FN Thomson Reuters Web of Science™
VR 1.0
PT J
AU Yu, HB
Remer, LA
Kahn, RA
Chin, M
Zhang, Y
AF Yu, Hongbin
Remer, Lorraine A.
Kahn, Ralph A.
Chin, Mian
Zhang, Yan
TI Satellite perspective of aerosol intercontinental transport: From
qualitative tracking to quantitative characterization
SO ATMOSPHERIC RESEARCH
LA English
DT Article
DE Aerosols; Particulate matter; Satellite remote sensing; Long-range
transport
ID RESOLUTION IMAGING SPECTRORADIOMETER; SUN PHOTOMETER MEASUREMENTS; SMOKE
INJECTION HEIGHTS; OPTICAL DEPTH RETRIEVAL; SAHARAN DUST TRANSPORT;
TO-BACKSCATTER RATIO; NORTH-AFRICAN DUST; FOREST-FIRE SMOKE;
AIR-POLLUTION; A-TRAIN
AB Evidence of aerosol intercontinental transport (ICT) is both widespread and compelling. Model simulations suggest that ICT could significantly affect regional air quality and climate, but the broad inter-model spread of results underscores a need of constraining model simulations with measurements. Satellites have inherent advantages over in situ measurements to characterize aerosol ICT, because of their spatial and temporal coverage. Significant progress in satellite remote sensing of aerosol properties during the Earth Observing System (EOS) era offers the opportunity to increase quantitative characterization and estimates of aerosol ICT beyond the capability of pre-EOS era satellites that could only qualitatively track aerosol plumes. EOS satellites also observe emission strengths and injection heights of some aerosols, aerosol precursors, and aerosol-related gases, which can help characterize aerosol ICT. We review how the current generation of satellite measurements have been used to (1) characterize the evolution of aerosol plumes (e.g., both horizontal and vertical transport, and properties) on an episodic basis, (2) understand the seasonal and inter-annual variations of aerosol ICT and their control factors, (3) estimate the export and import fluxes of aerosols, and (4) evaluate and constrain model simulations. Substantial effort is needed to further explore an integrated approach using measurements from on-orbit satellites (e.g., A-Train synergy) for observational characterization and model constraint of aerosol intercontinental transport and to develop advanced sensors for future missions. (C) 2013 Elsevier B.V. All rights reserved.
C1 [Yu, Hongbin] Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20740 USA.
[Yu, Hongbin; Kahn, Ralph A.; Chin, Mian; Zhang, Yan] NASA, Goddard Space Flight Ctr, Earth Sci Directorate, Greenbelt, MD 20771 USA.
[Remer, Lorraine A.] Univ Maryland Baltimore Cty, Joint Ctr Earth Syst Technol, Baltimore, MD 21228 USA.
[Zhang, Yan] Univ Space Res Assoc, Columbia, MD 21044 USA.
RP Yu, HB (reprint author), NASA, Goddard Space Flight Ctr, Climate & Radiat Lab, Code 613, Greenbelt, MD 20771 USA.
EM Hongbin.Yu@nasa.gov
RI Yu, Hongbin/C-6485-2008; Liu, Yanan/J-3680-2012; Chin, Mian/J-8354-2012;
Kahn, Ralph/D-5371-2012
OI Yu, Hongbin/0000-0003-4706-1575; Kahn, Ralph/0000-0002-5234-6359
FU NASA [NNXAH66G, NNX11AJ91G]; NASA Modeling
FX HY, LAR, MC, and YZ acknowledge the NASA support of this work via
NNXAH66G (The Science of Terra and Aqua program) and NNX11AJ91G
(Atmospheric Composition Modeling and Analysis - ACMAP program), both
managed by Richard Eckman. MC was also supported in part by NASA
Modeling, Analysis, and Projection program managed by David Considine.
The work of RK was supported in part by NASA's Climate and Radiation
Research and Analysis Program under Hal Maring, ACIVIAP program under
Richard Eckman, and the EOS-MISR instrument project. We thank anonymous
reviewers for insightful comments that have helped improve the quality
of the paper.
NR 266
TC 19
Z9 19
U1 4
U2 46
PU ELSEVIER SCIENCE INC
PI NEW YORK
PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA
SN 0169-8095
EI 1873-2895
J9 ATMOS RES
JI Atmos. Res.
PD APR 28
PY 2013
VL 124
BP 73
EP 100
DI 10.1016/j.atmosres.2012.12.013
PG 28
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 125QQ
UT WOS:000317556800007
ER
PT J
AU Pokhrel, YN
Fan, Y
Miguez-Macho, G
Yeh, PJF
Han, SC
AF Pokhrel, Yadu N.
Fan, Ying
Miguez-Macho, Gonzalo
Yeh, Pat J. -F.
Han, Shin-Chan
TI The role of groundwater in the Amazon water cycle: 3. Influence on
terrestrial water storage computations and comparison with GRACE
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
ID CLIMATE EXPERIMENT GRACE; SEQUENCE BENEATH FOREST; FLOODPLAIN LAKE;
GRAVITY RECOVERY; BASIN; HYDROLOGY; VARIABILITY; BEHAVIOR; BALANCE;
EVAPOTRANSPIRATION
AB We explore the mechanisms whereby groundwater influences terrestrial water storage (TWS) in the Amazon using GRACE observations and two contrasting versions of the LEAF-Hydro-Flood hydrological model: one with and the other without an interactive groundwater. We find that, first, where the water table is shallow as in northwestern Amazonia and floodplains elsewhere, subsurface stores (vadose zone and groundwater) are nearly saturated year-round, hence river and flooding dominate TWS variation; where the water table is deep as in southeastern Amazonia, the large subsurface storage capacity holds the infiltrated water longer before releasing it to streams, hence the subsurface storage dominates TWS variation. Second, over the whole Amazon, the subsurface water contribution far exceeds surface water contribution to total TWS variations. Based on LEAF-Hydro-Flood simulations, 71% of TWS change is from subsurface water, 24% from flood water, and 5% from water in river channels. Third, the subsurface store includes two competing terms, soil water in the vadose zone and groundwater below the water table. As the water table rises, the length of vadose zone is shortened and hence the change in groundwater store is accompanied by an opposite change in soil water store resulting in their opposite phase and contributions to total TWS. We conclude that the inclusion of a prognostic groundwater store and its interactions with the vadose zone, rivers, and floodplains in hydrological simulations enhances seasonal amplitudes and delays seasonal peaks of TWS anomaly, leading to an improved agreement with GRACE observations.
C1 [Pokhrel, Yadu N.; Fan, Ying] Rutgers State Univ, Dept Earth & Planetary Sci, New Brunswick, NJ 08854 USA.
[Miguez-Macho, Gonzalo] Univ Santiago de Compostela, Fac Phys, Nonlinear Phys Grp, Galicia, Spain.
[Yeh, Pat J. -F.] UNESCO, Int Ctr Water Hazard & Risk Management ICHARM, Tsukuba, Ibaraki, Japan.
[Han, Shin-Chan] NASA, Goddard Space Flight Ctr, Planetary Geodynam Lab, Greenbelt, MD 20771 USA.
RP Pokhrel, YN (reprint author), Rutgers State Univ, Dept Earth & Planetary Sci, New Brunswick, NJ 08854 USA.
EM yadupokhrel@eps.rutgers.edu
RI Han, Shin-Chan/A-2022-2009; Pokhrel, Yadu /J-6440-2013; YEH,
Pat/B-2758-2011
OI Pokhrel, Yadu /0000-0002-1367-216X; YEH, Pat/0000-0001-7629-3362
FU National Science Foundation; NASA's Earth Surface and Interior program;
GRACE projects; [NSF-AGS-1045110]; [EPA-STAR-RD834190]
FX Funding comes from NSF-AGS-1045110 and EPA-STAR-RD834190. Computation
support comes from CESGA (Centro de Supercomputacion de Galicia)
Supercomputer Center at the Universidade de Santiago de Compostela,
Galicia, Spain, and the Climate Simulation Laboratory at NCAR's
Computational and Information Systems Laboratory, sponsored by the
National Science Foundation and other agencies. SCH is supported by
NASA's Earth Surface and Interior program and GRACE projects.
NR 72
TC 24
Z9 24
U1 1
U2 41
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-897X
EI 2169-8996
J9 J GEOPHYS RES-ATMOS
JI J. Geophys. Res.-Atmos.
PD APR 27
PY 2013
VL 118
IS 8
BP 3233
EP 3244
DI 10.1002/jgrd.50335
PG 12
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 155JQ
UT WOS:000319744200016
ER
PT J
AU Zhu, L
Henze, DK
Cady-Pereira, KE
Shephard, MW
Luo, M
Pinder, RW
Bash, JO
Jeong, GR
AF Zhu, L.
Henze, D. K.
Cady-Pereira, K. E.
Shephard, M. W.
Luo, M.
Pinder, R. W.
Bash, J. O.
Jeong, G. -R.
TI Constraining U.S. ammonia emissions using TES remote sensing
observations and the GEOS-Chem adjoint model
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
ID AIR-QUALITY MODELS; UNITED-STATES; PART II; NITROGEN; POLLUTION;
NITRATE; TRENDS; PM2.5; VARIABILITY; SENSITIVITY
AB Ammonia (NH3) has significant impacts on biodiversity, eutrophication, and acidification. Widespread uncertainty in the magnitude and seasonality of NH3 emissions hinders efforts to address these issues. In this work, we constrain U. S. NH3 sources using observations from the TES satellite instrument with the GEOS-Chem model and its adjoint. The inversion framework is first validated using simulated observations. We then assimilate TES observations for April, July, and October of 2006 through 2009. The adjoint-based inversion allows emissions to be adjusted heterogeneously; they are found to increase in California throughout the year, increase in different regions of the West depending upon season, and exhibit smaller increases and occasional decreases in the Eastern U. S. Evaluations of the inversion using independent surface measurements show reduced model underestimates of surface NH3 and wet deposited NHx in April and October; however, the constrained simulation in July leads to overestimates of these quantities, while TES observations are still under predicted. Modeled sulfate and nitrate aerosols concentrations do not change significantly, and persistent nitrate overestimation is noted, consistent with previous studies. Overall, while satellite-based constraints on NH3 emissions improve model simulations in several aspects, additional assessment at higher horizontal resolution of spatial sampling bias, nitric acid formation, and diurnal variability and bi-directionality of NH3 sources may be necessary to enhance year-round model performance across the full range of gas and aerosol evaluations.
C1 [Zhu, L.; Henze, D. K.; Jeong, G. -R.] Univ Colorado, Dept Mech Engn, Boulder, CO 80309 USA.
[Cady-Pereira, K. E.] Atmospher & Environm Res Inc, Lexington, MA USA.
[Shephard, M. W.] Atmospher & Climate Applicat Inc, East Gwillimbury, ON, Canada.
[Shephard, M. W.] Environm Canada, Toronto, ON, Canada.
[Luo, M.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Pinder, R. W.; Bash, J. O.; Jeong, G. -R.] US EPA, Res Triangle Pk, NC 27711 USA.
RP Henze, DK (reprint author), Univ Colorado, Dept Mech Engn, Boulder, CO 80309 USA.
EM daven.henze@colorado.edu
RI Bash, Jesse/E-9688-2013; Pinder, Robert/F-8252-2011; Chem,
GEOS/C-5595-2014;
OI Pinder, Robert/0000-0001-6390-7126; Bash, Jesse/0000-0001-8736-0102
FU NASA [NNX09AN77G, NNX10AG63G]; EPA STAR [RD834559]
FX This work is supported by NASA grants NNX09AN77G and NNX10AG63G and EPA
STAR award RD834559. While this manuscript has been reviewed by the
Environmental Protection Agency and approved for publication, it may not
reflect official agency views or policies.
NR 58
TC 41
Z9 42
U1 5
U2 39
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-897X
EI 2169-8996
J9 J GEOPHYS RES-ATMOS
JI J. Geophys. Res.-Atmos.
PD APR 27
PY 2013
VL 118
IS 8
BP 3355
EP 3368
DI 10.1002/jgrd.50166
PG 14
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 155JQ
UT WOS:000319744200028
ER
PT J
AU Tiscareno, MS
Mitchell, CJ
Murray, CD
Di Nino, D
Hedman, MM
Schmidt, J
Burns, JA
Cuzzi, JN
Porco, CC
Beurle, K
Evans, MW
AF Tiscareno, Matthew S.
Mitchell, Colin J.
Murray, Carl D.
Di Nino, Daiana
Hedman, Matthew M.
Schmidt, Juergen
Burns, Joseph A.
Cuzzi, Jeffrey N.
Porco, Carolyn C.
Beurle, Kevin
Evans, Michael W.
TI Observations of Ejecta Clouds Produced by Impacts onto Saturn's Rings
SO SCIENCE
LA English
DT Article
ID F RING; BOMBARDMENT
AB We report observations of dusty clouds in Saturn's rings, which we interpret as resulting from impacts onto the rings that occurred between 1 and 50 hours before the clouds were observed. The largest of these clouds was observed twice; its brightness and cant angle evolved in a manner consistent with this hypothesis. Several arguments suggest that these clouds cannot be due to the primary impact of one solid meteoroid onto the rings, but rather are due to the impact of a compact stream of Saturn-orbiting material derived from previous breakup of a meteoroid. The responsible interplanetary meteoroids were initially between 1 centimeter and several meters in size, and their influx rate is consistent with the sparse prior knowledge of smaller meteoroids in the outer solar system.
C1 [Tiscareno, Matthew S.; Hedman, Matthew M.; Evans, Michael W.] Cornell Univ, Ctr Radiophys & Space Res, Ithaca, NY 14853 USA.
[Mitchell, Colin J.; Di Nino, Daiana; Porco, Carolyn C.] Space Sci Inst, CICLOPS, Boulder, CO 80301 USA.
[Murray, Carl D.; Beurle, Kevin] Queen Mary Univ London, Astron Unit, London E1 4NS, England.
[Schmidt, Juergen] Univ Oulu, Dept Phys, Astron Div, FI-90014 Oulu, Finland.
[Schmidt, Juergen] Univ Potsdam, Inst Phys & Astron, D-14476 Potsdam, Germany.
[Burns, Joseph A.] Cornell Univ, Dept Astron, Ithaca, NY 14853 USA.
[Burns, Joseph A.] Cornell Univ, Coll Engn, Ithaca, NY 14853 USA.
[Cuzzi, Jeffrey N.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
RP Tiscareno, MS (reprint author), Cornell Univ, Ctr Radiophys & Space Res, Ithaca, NY 14853 USA.
EM matthewt@astro.cornell.edu
FU NASA Cassini Data Analysis program [NNX08AQ72G, NNX10AG67G]; Cassini
project; Science and Technology Facilities Council [ST/F007566/1]
FX We thank M. Showalter for helpful discussions and for the use of Mie
scattering code. We thank the Cassini project and the Cassini Imaging
Team for making these observations possible. M. S. T. acknowledges
funding from the NASA Cassini Data Analysis program (NNX08AQ72G and
NNX10AG67G) and the Cassini project. C. D. M. acknowledges funding from
the Science and Technology Facilities Council (grant ST/F007566/1).
NR 21
TC 11
Z9 11
U1 1
U2 11
PU AMER ASSOC ADVANCEMENT SCIENCE
PI WASHINGTON
PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 USA
SN 0036-8075
J9 SCIENCE
JI Science
PD APR 26
PY 2013
VL 340
IS 6131
BP 460
EP 464
DI 10.1126/science.1233524
PG 5
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 131SQ
UT WOS:000318016700037
PM 23620048
ER
PT J
AU Bhatia, AK
AF Bhatia, A. K.
TI Hybrid theory of P-wave electron-Li2+ elastic scattering and
photoabsorption in two-electron systems
SO PHYSICAL REVIEW A
LA English
DT Article
ID PHOTOIONIZATION CROSS-SECTIONS; PHASE-SHIFTS; HYDROGEN; HE;
PHOTODETACHMENT; HELIUM; RESONANCES; ENERGIES; FEEDBACK; STATES
AB In previous papers [Bhatia, Phys. Rev. A 85, 052708 (2012); 86, 032709 (2012)] electron-hydrogen and electron-He+ P-wave scattering phase shifts were calculated using the hybrid theory. This method is extended to the singlet and triplet electron-Li2+ P-wave scattering in the elastic region, where the correlation functions are of Hylleraas type. The short-range and long-range correlations are included in the Schrodinger equation at the same time, by using a combination of a modified method of polarized orbitals and the optical potential formalism. Phase shifts are compared to those obtained by other methods. The present calculation requires very few correlation functions to obtain accurate results which are rigorous lower bounds to the exact phase shifts. The continuum functions obtained in this method are used to calculate photodetachment and photoionization cross sections of two-electron systems H-, He, and Li+. Cross sections of the metastable S-1,S-3 states of He, and Li+ are also calculated. These cross sections are calculated in the elastic region and compared with previous calculations. Using these cross sections, the Maxwellian-averaged radiative-recombination rates at various electron temperatures are also calculated. DOI: 10.1103/PhysRevA.87.042705
C1 NASA, Goddard Space Flight Ctr, Heliophys Sci Div, Greenbelt, MD 20771 USA.
RP Bhatia, AK (reprint author), NASA, Goddard Space Flight Ctr, Heliophys Sci Div, Greenbelt, MD 20771 USA.
NR 37
TC 4
Z9 4
U1 1
U2 11
PU AMER PHYSICAL SOC
PI COLLEGE PK
PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA
SN 1050-2947
J9 PHYS REV A
JI Phys. Rev. A
PD APR 25
PY 2013
VL 87
IS 4
AR 042705
DI 10.1103/PhysRevA.87.042705
PG 9
WC Optics; Physics, Atomic, Molecular & Chemical
SC Optics; Physics
GA 133XC
UT WOS:000318173200006
ER
PT J
AU Galley, CR
Behunin, RO
Hu, BL
AF Galley, Chad R.
Behunin, Ryan O.
Hu, B. L.
TI Oscillator-field model of moving mirrors in quantum optomechanics
SO PHYSICAL REVIEW A
LA English
DT Article
ID RESOLVED-SIDE-BAND; ELECTROMAGNETIC-FIELD; MICROMECHANICAL OSCILLATOR;
RADIATION-PRESSURE; PARTICLE CREATION; DIMENSIONAL SPACE; DISPERSIVE
MIRROR; STATE REDUCTION; MASTER EQUATION; BROWNIAN-MOTION
AB We present a microphysics model for the kinematics and dynamics of optomechanics describing the coupling between an optical field, modeled here by a massless scalar field, and the internal and mechanical degrees of freedom of a movable mirror. Instead of implementing boundary conditions on the field, we introduce an internal degree of freedom and its dynamics to describe the mirror's reflectivity. Depending on parameter values, the internal degrees of freedom of the mirror in this model capture a range of its optical activities, from those exhibiting broadband reflective properties to those reflecting only in a narrow band. After establishing the model we show how appropriate parameter choices lead to other well-known optomechanical models, including those of Barton and Calogeracos [Ann. Phys. (NY) 238, 227 (1995)], Calogeracos and Barton, Ann. Phys. (NY) 238, 268 (1995), Law [Phys. Rev. A 51, 2537 (1995)], and Golestanian and Kardar [Phys. Rev. Lett. 78, 3421 (1997); Phys. Rev. A 58, 1713 (1998)]. As a simple illustrative application we derive classical radiation pressure cooling from this model. We then connect our microphysics model to the common descriptions of a moving mirror coupled to radiation pressure (e. g., with Nx coupling, where N is the photon number and x is the mirror displacement), making explicit the underlying assumptions made in these phenomenological models. Our model is also applicable to the lesser explored case of small N, which existing models based on sideband approximations [Kimble et al., Phys. Rev. D 65, 022002 (2001)] have not addressed. Interestingly, we also find that slow-moving mirrors in our model can be described by the ubiquitous Brownian motion model of quantum open systems. The scope of applications of this model ranges from a full quantum-mechanical treatment of radiation pressure cooling and quantum entanglement between macroscopic mirrors to the back reaction of Hawking radiation on black-hole evaporation in a moving mirror analog. DOI: 10.1103/PhysRevA.87.043832
C1 [Galley, Chad R.] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
[Galley, Chad R.] CALTECH, Pasadena, CA 91106 USA.
[Behunin, Ryan O.] Los Alamos Natl Lab, Ctr Nonlinear Studies, Los Alamos, NM 87545 USA.
[Behunin, Ryan O.] Los Alamos Natl Lab, Div Theoret, Los Alamos, NM 87545 USA.
[Hu, B. L.] Univ Maryland, Joint Quantum Inst, College Pk, MD 20742 USA.
[Hu, B. L.] Univ Maryland, Maryland Ctr Fundamental Phys, College Pk, MD 20742 USA.
[Hu, B. L.] Hong Kong Univ Sci & Technol, Inst Adv Study, Kowloon, Hong Kong, Peoples R China.
[Hu, B. L.] Hong Kong Univ Sci & Technol, Dept Phys, Kowloon, Hong Kong, Peoples R China.
RP Galley, CR (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91125 USA.
FU NASA; NIST Gaithersburg grant; US Department of Energy through the LANL
LDRD program; NSF [PHY-0801368]
FX C.G. was supported in part by an appointment to the NASA Postdoctoral
Program at the Jet Propulsion Laboratory administered by Oak Ridge
Associated Universities through a contract with NASA and in part by a
NIST Gaithersburg grant awarded to the University of Maryland when this
work was started. R. B. gratefully acknowledges the support of the US
Department of Energy through the LANL LDRD program. B. L. H. wishes to
thank Prof. Jason Twamley, director of the Centre for Quantum Computer
Technology at Macquarie University, for his warm hospitality in
February-March 2011 during which this work was partly carried out. His
research was partially supported by NSF Grant No. PHY-0801368 to the
University of Maryland.
NR 101
TC 3
Z9 3
U1 2
U2 16
PU AMER PHYSICAL SOC
PI COLLEGE PK
PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA
SN 1050-2947
J9 PHYS REV A
JI Phys. Rev. A
PD APR 24
PY 2013
VL 87
IS 4
AR 043832
DI 10.1103/PhysRevA.87.043832
PG 21
WC Optics; Physics, Atomic, Molecular & Chemical
SC Optics; Physics
GA 131AV
UT WOS:000317963700006
ER
PT J
AU Hansen, J
Sato, M
Ruedy, R
AF Hansen, James
Sato, Makiko
Ruedy, Reto
TI Reply to Stone et al.: Human-made role in local temperature extremes
SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF
AMERICA
LA English
DT Letter
C1 [Hansen, James; Sato, Makiko] NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
[Hansen, James; Sato, Makiko] Columbia Univ, Earth Inst, New York, NY 10025 USA.
[Ruedy, Reto] Trinnovim LLC, New York, NY 10025 USA.
RP Hansen, J (reprint author), NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
EM james.e.hansen@nasa.gov
NR 4
TC 3
Z9 3
U1 0
U2 8
PU NATL ACAD SCIENCES
PI WASHINGTON
PA 2101 CONSTITUTION AVE NW, WASHINGTON, DC 20418 USA
SN 0027-8424
J9 P NATL ACAD SCI USA
JI Proc. Natl. Acad. Sci. U. S. A.
PD APR 23
PY 2013
VL 110
IS 17
BP E1544
EP E1544
DI 10.1073/pnas.1301494110
PG 1
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 140TE
UT WOS:000318677300002
PM 23745185
ER
PT J
AU Galley, CR
AF Galley, Chad R.
TI Classical Mechanics of Nonconservative Systems
SO PHYSICAL REVIEW LETTERS
LA English
DT Article
AB Hamilton's principle of stationary action lies at the foundation of theoretical physics and is applied in many other disciplines from pure mathematics to economics. Despite its utility, Hamilton's principle has a subtle pitfall that often goes unnoticed in physics: it is formulated as a boundary value problem in time but is used to derive equations of motion that are solved with initial data. This subtlety can have undesirable effects. I present a formulation of Hamilton's principle that is compatible with initial value problems. Remarkably, this leads to a natural formulation for the Lagrangian and Hamiltonian dynamics of generic nonconservative systems, thereby filling a long-standing gap in classical mechanics. Thus, dissipative effects, for example, can be studied with new tools that may have applications in a variety of disciplines. The new formalism is demonstrated by two examples of nonconservative systems: an object moving in a fluid with viscous drag forces and a harmonic oscillator coupled to a dissipative environment. DOI: 10.1103/PhysRevLett.110.174301
C1 [Galley, Chad R.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Galley, Chad R.] CALTECH, Pasadena, CA 91125 USA.
RP Galley, CR (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM crgalley@tapir.caltech.edu
FU Jet Propulsion Laboratory
FX I thank Y. Chen, C. Cutler, K. Hawbaker, A. Leibovich, H. Miao, E.
Poisson, I. Rothstein, G. Schafer, L. Stein, A. Tolley, M. Vallisneri,
and especially A. Zenginoglu for discussions and comments of previous
drafts. This work was supported in part by an appointment to the NASA
Postdoctoral Program at the Jet Propulsion Laboratory administered by
the Oak Ridge Associated Universities through a contract with NASA.
NR 15
TC 45
Z9 45
U1 0
U2 18
PU AMER PHYSICAL SOC
PI COLLEGE PK
PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA
SN 0031-9007
J9 PHYS REV LETT
JI Phys. Rev. Lett.
PD APR 22
PY 2013
VL 110
IS 17
AR 174301
DI 10.1103/PhysRevLett.110.174301
PG 5
WC Physics, Multidisciplinary
SC Physics
GA 129CK
UT WOS:000317815800009
PM 23679733
ER
PT J
AU Cantrell, JH
Yost, WT
AF Cantrell, John H.
Yost, William T.
TI Acoustic nonlinearity and cumulative plastic shear strain in cyclically
loaded metals
SO JOURNAL OF APPLIED PHYSICS
LA English
DT Article
ID WAVY SLIP METALS; HARMONIC-GENERATION; ULTRASONIC-WAVES; FATIGUE DAMAGE
AB Cyclic loading leads to microstructural changes in metals that result in substantial increases in the material nonlinearity. Two quite distinct approaches for quantifying the nonlinearity via a material nonlinearity parameter assessed directly from acoustic harmonic generation measurements have emerged-the Cantrell model and the model of Kim et al. The Cantrell model quantifies the nonlinearity in terms of lattice anharmonicity, dislocation plasticity, and crack growth as independent sources of nonlinearity arising from the accumulated plastic shear strain. The approach of Kim et al. links the cumulative plastic shear strain directly to a change in the third-order elastic constants of the material. We show that although the model of Kim et al. has the advantage of expediency, the Cantrell model reflects much more accurately the dependence of the nonlinearity parameter on the state of fatigue.
C1 [Cantrell, John H.; Yost, William T.] NASA, Res Directorate, Langley Res Ctr, Hampton, VA 23681 USA.
RP Cantrell, JH (reprint author), NASA, Res Directorate, Langley Res Ctr, Hampton, VA 23681 USA.
EM john.h.cantrell@nasa.gov; William.t.yost@nasa.gov
NR 19
TC 8
Z9 9
U1 0
U2 14
PU AMER INST PHYSICS
PI MELVILLE
PA CIRCULATION & FULFILLMENT DIV, 2 HUNTINGTON QUADRANGLE, STE 1 N O 1,
MELVILLE, NY 11747-4501 USA
SN 0021-8979
J9 J APPL PHYS
JI J. Appl. Phys.
PD APR 21
PY 2013
VL 113
IS 15
AR 153506
DI 10.1063/1.4801885
PG 6
WC Physics, Applied
SC Physics
GA 134YJ
UT WOS:000318251400012
ER
PT J
AU Dobler, JT
Harrison, FW
Browell, EV
Lin, B
McGregor, D
Kooi, S
Choi, Y
Ismail, S
AF Dobler, Jeremy T.
Harrison, F. Wallace
Browell, Edward V.
Lin, Bing
McGregor, Doug
Kooi, Susan
Choi, Yonghoon
Ismail, Syed
TI Atmospheric CO2 column measurements with an airborne intensity-modulated
continuous wave 1.57 mu m fiber laser lidar
SO APPLIED OPTICS
LA English
DT Article
ID DIFFERENTIAL ABSORPTION LIDAR; CARBON-DIOXIDE; CW LIDAR; SYSTEM; SPACE
AB The 2007 National Research Council (NRC) Decadal Survey on Earth Science and Applications from Space recommended Active Sensing of CO2 Emissions over Nights, Days, and Seasons (ASCENDS) as a midterm, Tier II, NASA space mission. ITT Exelis, formerly ITT Corp., and NASA Langley Research Center have been working together since 2004 to develop and demonstrate a prototype laser absorption spectrometer for making high-precision, column CO2 mixing ratio measurements needed for the ASCENDS mission. This instrument, called the multifunctional fiber laser lidar (MFLL), operates in an intensity-modulated, continuous wave mode in the 1.57 mu m CO2 absorption band. Flight experiments have been conducted with the MFLL on a Lear-25, UC-12, and DC-8 aircraft over a variety of different surfaces and under a wide range of atmospheric conditions. Very high-precision CO2 column measurements resulting from high signal-to-noise ratio (>1300) column optical depth (OD) measurements for a 10 s (similar to 1 km) averaging interval have been achieved. In situ measurements of atmospheric CO2 profiles were used to derive the expected CO2 column values, and when compared to the MFLL measurements over desert and vegetated surfaces, the MFLL measurements were found to agree with the in situ-derived CO2 columns to within an average of 0.17% or similar to 0.65 ppmv with a standard deviation of 0.44% or similar to 1.7 ppmv. Initial results demonstrating ranging capability using a swept modulation technique are also presented. (C) 2013 Optical Society of America
C1 [Dobler, Jeremy T.; McGregor, Doug] Exelis Inc, Ft Wayne, IN 46818 USA.
[Harrison, F. Wallace; Lin, Bing; Ismail, Syed] NASA, Langley Res Ctr, Hampton, VA 23681 USA.
[Browell, Edward V.] NASA, Langley Res Ctr, STARSS Affiliate 2, Hampton, VA 23681 USA.
[Kooi, Susan; Choi, Yonghoon] Sci Syst & Applicat Inc, Hampton, VA 23666 USA.
RP Dobler, JT (reprint author), Exelis Inc, 1919 W Cook Rd, Ft Wayne, IN 46818 USA.
EM Jeremy.Dobler@exelisinc.com
NR 43
TC 35
Z9 35
U1 4
U2 25
PU OPTICAL SOC AMER
PI WASHINGTON
PA 2010 MASSACHUSETTS AVE NW, WASHINGTON, DC 20036 USA
SN 1559-128X
J9 APPL OPTICS
JI Appl. Optics
PD APR 20
PY 2013
VL 52
IS 12
BP 2874
EP 2892
DI 10.1364/AO.52.002874
PG 19
WC Optics
SC Optics
GA 130NB
UT WOS:000317923700044
PM 23669700
ER
PT J
AU Sorek-Hamer, M
Cohen, A
Levy, RC
Ziv, B
Broday, DM
AF Sorek-Hamer, M.
Cohen, A.
Levy, R. C.
Ziv, B.
Broday, D. M.
TI Classification of dust days by satellite remotely sensed aerosol
products
SO INTERNATIONAL JOURNAL OF REMOTE SENSING
LA English
DT Article
ID FINE PARTICULATE MATTER; GROUND-BASED MEASUREMENTS; AIR-POLLUTION;
OPTICAL DEPTH; PREDICTION SYSTEM; DAILY MORTALITY; HEART-DISEASE; MODIS;
QUALITY; PM2.5
AB Considerable progress in satellite remote sensing (SRS) of dust particles has been seen in the last decade. From an environmental health perspective, such an event detection, after linking it to ground particulate matter (PM) concentrations, can proxy acute exposure to respirable particles of certain properties (i.e. size, composition, and toxicity). Being affected considerably by atmospheric dust, previous studies in the Eastern Mediterranean, and in Israel in particular, have focused on mechanistic and synoptic prediction, classification, and characterization of dust events. In particular, a scheme for identifying dust days (DD) in Israel based on ground PM10 (particulate matter of size smaller than 10 m) measurements has been suggested, which has been validated by compositional analysis. This scheme requires information regarding ground PM10 levels, which is naturally limited in places with sparse ground-monitoring coverage. In such cases, SRS may be an efficient and cost-effective alternative to ground measurements. This work demonstrates a new model for identifying DD and non-DD (NDD) over Israel based on an integration of aerosol products from different satellite platforms (Moderate Resolution Imaging Spectroradiometer (MODIS) and Ozone Monitoring Instrument (OMI)). Analysis of ground-monitoring data from 2007 to 2008 in southern Israel revealed 67 DD, with more than 88% occurring during winter and spring. A Classification and Regression Tree (CART) model that was applied to a database containing ground monitoring (the dependent variable) and SRS aerosol product (the independent variables) records revealed an optimal set of binary variables for the identification of DD. These variables are combinations of the following primary variables: the calendar month, ground-level relative humidity (RH), the aerosol optical depth (AOD) from MODIS, and the aerosol absorbing index (AAI) from OMI. A logistic regression that uses these variables, coded as binary variables, demonstrated 93.2% correct classifications of DD and NDD. Evaluation of the combined CARTlogistic regression scheme in an adjacent geographical region (Gush Dan) demonstrated good results. Using SRS aerosol products for DD and NDD, identification may enable us to distinguish between health, ecological, and environmental effects that result from exposure to these distinct particle populations.
C1 [Sorek-Hamer, M.; Cohen, A.; Broday, D. M.] Technion Israel Inst Technol, Haifa, Israel.
[Levy, R. C.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Ziv, B.] Open Univ Israel, Raanana, Israel.
RP Broday, DM (reprint author), Technion Israel Inst Technol, Haifa, Israel.
EM dbroday@tx.technion.ac.il
RI Levy, Robert/M-7764-2013;
OI Levy, Robert/0000-0002-8933-5303; Broday, David/0000-0002-6525-3979
FU Israel Ministry of Science and Technology; Israel Council for Higher
Education
FX MSH was supported by scholarships from the Israel Ministry of Science
and Technology and from the Israel Council for Higher Education. Data
were obtained from the Goddard Earth Science Data Center in NASA GSFC,
Israel Ministry of Environment Protection, Israel Electric Company, and
the Ashdod-Ashkelon Association of Municipalities for the Environment.
The study was done within the Technion Center of Excellence in Exposure
Science and Environmental Health (TCEEH).
NR 56
TC 8
Z9 8
U1 1
U2 26
PU TAYLOR & FRANCIS LTD
PI ABINGDON
PA 4 PARK SQUARE, MILTON PARK, ABINGDON OX14 4RN, OXON, ENGLAND
SN 0143-1161
J9 INT J REMOTE SENS
JI Int. J. Remote Sens.
PD APR 20
PY 2013
VL 34
IS 8
BP 2672
EP 2688
DI 10.1080/01431161.2012.748991
PG 17
WC Remote Sensing; Imaging Science & Photographic Technology
SC Remote Sensing; Imaging Science & Photographic Technology
GA 109UG
UT WOS:000316393800002
ER
PT J
AU O'Connell, J
Connolly, J
Vermote, EF
Holden, NM
AF O'Connell, Jerome
Connolly, John
Vermote, Eric F.
Holden, Nicholas M.
TI Radiometric normalization for change detection in peatlands: a modified
temporal invariant cluster approach
SO INTERNATIONAL JOURNAL OF REMOTE SENSING
LA English
DT Article
ID ENHANCED VEGETATION INDEX; REPUBLIC-OF-IRELAND; LAND-COVER CHANGE;
CARBON STOCKS; TIME-SERIES; IMAGERY; MODIS; REFLECTANCE; REMOTE
AB Radiometric normalization is a vital stage in any change detection study due to the complex interactions of radiance and irradiance between the Earth's surface and atmosphere. Compensation for variables such as sun's angle, surface profile, atmospheric conditions, and sensor calibration coefficients are essential in achieving a radiometrically stable data base of multi-temporal, multi-spectral imagery for a change detection study. In this study, five Landsat Enhanced Thematic Mapper Plus (ETM+) images taken over the east coast of Ireland in 2001 were geometrically corrected and topographically normalized for further processing and analysis. Assessment of various vegetation indices showed that the enhanced vegetation index 2 (EVI2) gave the highest accuracy in identifying the various vegetation types and habitats in the Wicklow Mountains National Park. The initial analysis of radiometric normalization with temporal invariant clusters (TICs) gave poor results due to the spectral heterogeneity of urban pixels within each image. A revised TIC subset normalized method was developed using regional growth parameters in urban environments to limit the spatial and spectral extent of pixels used in the TIC scene normalization process. Correlation analysis between the TIC-subset-normalized ETM+ data and Landsat Ecosystem Disturbance Adaptive Processing System (LEDAPS) absolute corrected data produced coefficient of determination (R-2) values between 0.88 and 0.98. Such results demonstrated the robustness of the TIC subset normalization procedure when correcting for atmospheric variability between images while maintaining spectral integrity. Statistical analysis on master slave and TIC-subset-normalized slave data using cumulative distribution curves derived from image histograms showed an 86.93% reduction in the maximum difference between master and slave data due to the TIC subset normalization process. This procedure of radiometric normalization is suitable in landscapes with a low density of spectrally stable targets.
C1 [O'Connell, Jerome; Holden, Nicholas M.] Natl Univ Ireland Univ Coll Dublin, Sch Biosyst Engn, Agr & Food Sci Ctr, Dublin 4, Ireland.
[Connolly, John] Natl Univ Ireland Univ Coll Cork, Dept Geog, Cork, Ireland.
[Vermote, Eric F.] NASA, Goddard Space Flight Ctr, Terr Informat Syst Branch, Greenbelt, MD 20771 USA.
RP O'Connell, J (reprint author), Univ Leeds, Fac Biol Sci, Sch Biol, Leeds LS2 9JT, W Yorkshire, England.
EM J.O'Connell@leeds.ac.uk
RI Connolly, John/A-2925-2014; Connolly, John/A-8976-2013; O Connell,
Jerome/M-6517-2014
OI Connolly, John/0000-0002-2897-9711; Connolly, John/0000-0002-2897-9711;
O Connell, Jerome/0000-0002-4782-1549
FU Environmental Protection Agency of Ireland (EPA) under the STRIVE
fellowship
FX The authors wish to thank the Environmental Protection Agency of Ireland
(EPA) for their financial support under the STRIVE fellowship. The
authors also wish to thank the US Geological Survey for providing access
to the ETM+ data, as well as the NPWS for supplying habitat maps of the
Wicklow Mountains National Park.
NR 53
TC 6
Z9 6
U1 0
U2 13
PU TAYLOR & FRANCIS LTD
PI ABINGDON
PA 4 PARK SQUARE, MILTON PARK, ABINGDON OX14 4RN, OXON, ENGLAND
SN 0143-1161
J9 INT J REMOTE SENS
JI Int. J. Remote Sens.
PD APR 20
PY 2013
VL 34
IS 8
BP 2905
EP 2924
DI 10.1080/01431161.2012.752886
PG 20
WC Remote Sensing; Imaging Science & Photographic Technology
SC Remote Sensing; Imaging Science & Photographic Technology
GA 109UG
UT WOS:000316393800014
ER
PT J
AU Bentz, MC
Denney, KD
Grier, CJ
Barth, AJ
Peterson, BM
Vestergaard, M
Bennert, VN
Canalizo, G
De Rosa, G
Filippenko, AV
Gates, EL
Greene, JE
Li, WD
Malkan, MA
Pogge, RW
Stern, D
Treu, T
Woo, JH
AF Bentz, Misty C.
Denney, Kelly D.
Grier, Catherine J.
Barth, Aaron J.
Peterson, Bradley M.
Vestergaard, Marianne
Bennert, Vardha N.
Canalizo, Gabriela
De Rosa, Gisella
Filippenko, Alexei V.
Gates, Elinor L.
Greene, Jenny E.
Li, Weidong
Malkan, Matthew A.
Pogge, Richard W.
Stern, Daniel
Treu, Tommaso
Woo, Jong-Hak
TI THE LOW-LUMINOSITY END OF THE RADIUS-LUMINOSITY RELATIONSHIP FOR ACTIVE
GALACTIC NUCLEI
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: active; galaxies: nuclei; galaxies: photometry; galaxies:
Seyfert
ID BROAD-LINE REGION; BLACK-HOLE MASSES; SEYFERT 1 GALAXIES; REVERBERATION
MAPPING DATA; BRIGHT QUASAR SURVEY; HOST-GALAXY; COSMIC EVOLUTION;
INTRINSIC SCATTER; SCALING RELATIONS; ASTRONOMICAL DATA
AB We present an updated and revised analysis of the relationship between the H beta broad-line region (BLR) radius and the luminosity of the active galactic nucleus (AGN). Specifically, we have carried out two-dimensional surface brightness decompositions of the host galaxies of nine new AGNs imaged with the Hubble Space Telescope Wide Field Camera 3. The surface brightness decompositions allow us to create "AGN-free" images of the galaxies, from which we measure the starlight contribution to the optical luminosity measured through the ground-based spectroscopic aperture. We also incorporate 20 new reverberation-mapping measurements of the H beta time lag, which is assumed to yield the average H beta BLR radius. The final sample includes 41 AGNs covering four orders of magnitude in luminosity. The additions and updates incorporated here primarily affect the low-luminosity end of the R-BLR-L relationship. The best fit to the relationship using a Bayesian analysis finds a slope of alpha = 0.533(-0.033)(+0.035), consistent with previous work and with simple photoionization arguments. Only two AGNs appear to be outliers from the relationship, but both of them have monitoring light curves that raise doubt regarding the accuracy of their reported time lags. The scatter around the relationship is found to be 0.19 +/- 0.02 dex, but would be decreased to 0.13 dex by the removal of these two suspect measurements. A large fraction of the remaining scatter in the relationship is likely due to the inaccurate distances to the AGN host galaxies. Our results help support the possibility that the R-BLR-L relationship could potentially be used to turn the BLRs of AGNs into standardizable candles. This would allow the cosmological expansion of the universe to be probed by a separate population of objects, and over a larger range of redshifts.
C1 [Bentz, Misty C.] Georgia State Univ, Dept Phys & Astron, Atlanta, GA 30303 USA.
[Denney, Kelly D.; Vestergaard, Marianne] Niels Bohr Inst, Dark Cosmol Ctr, DK-2100 Copenhagen O, Denmark.
[Grier, Catherine J.; Peterson, Bradley M.; De Rosa, Gisella; Pogge, Richard W.] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA.
[Barth, Aaron J.] Univ Calif Irvine, Dept Phys & Astron, Irvine, CA 92697 USA.
[Peterson, Bradley M.; Pogge, Richard W.] Ohio State Univ, Ctr Cosmol & AstroParticle Phys, Columbus, OH 43210 USA.
[Vestergaard, Marianne] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA.
[Bennert, Vardha N.] Calif Polytech State Univ San Luis Obispo, Dept Phys, San Luis Obispo, CA 93407 USA.
[Canalizo, Gabriela] Univ Calif Riverside, Dept Phys & Astron, Riverside, CA 92521 USA.
[Filippenko, Alexei V.; Li, Weidong] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA.
[Gates, Elinor L.] Univ Calif Observ Lick Observ, Mt Hamilton, CA 95140 USA.
[Greene, Jenny E.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA.
[Malkan, Matthew A.] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA.
[Stern, Daniel] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Treu, Tommaso] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA.
[Woo, Jong-Hak] Seoul Natl Univ, Dept Phys & Astron, Astron Program, Seoul, South Korea.
RP Bentz, MC (reprint author), Georgia State Univ, Dept Phys & Astron, Atlanta, GA 30303 USA.
EM bentz@chara.gsu.edu
RI Woo, Jong-Hak/A-2790-2014; Vestergaard, Marianne/M-5247-2014;
OI Vestergaard, Marianne/0000-0001-9191-9837; Barth,
Aaron/0000-0002-3026-0562
FU Space Telescope Science Institute [HST GO-11662]; NASA [NAS5-26555];
European Union [300553]; NSF [AST-1108835, AST-1008882, AST-1108665,
AST-1211916]; TABASGO Foundation; Christopher R. Redlich Fund; National
Research Foundation of Korea (NRF); Korean government [2012-006087]
FX This work is based on observations with the NASA/ESA Hubble Space
Telescope. We are grateful for support of this work through grant HST
GO-11662 from the Space Telescope Science Institute, which is operated
by the Association of Universities for Research in Astronomy, Inc.,
under NASA contract NAS5-26555. K.D.D. has received funding from the
People Programme (Marie Curie Actions) of the European Union's Seventh
Framework Programme FP7/2007-2013/ under REA grant agreement No. 300553.
A.J.B. acknowledges support from NSF grant AST-1108835. B.M.P., C.J.G.,
G.D.R., and R.W.P. acknowledge support from NSF grant AST-1008882 to
Ohio State University. A.V.F. is grateful for the support of NSF grants
AST-1108665 and AST-1211916, the TABASGO Foundation, and the Christopher
R. Redlich Fund. The work of D.S. was carried out at Jet Propulsion
Laboratory, California Institute of Technology, under a contract with
NASA. J.H.W. acknowledges the support by the National Research
Foundation of Korea (NRF) grant funded by the Korean government (No.
2012-006087). This research has made use of the NASA/IPAC Extragalactic
Database (NED) which is operated by the Jet Propulsion Laboratory,
California Institute of Technology, under contract with the National
Aeronautics and Space Administration and the SIMBAD database, operated
at CDS, Strasbourg, France. We dedicate this paper to the memory of our
dear friend and colleague, Weidong Li, whose tireless dedication to the
Katzman Automatic Imaging Telescope (KAIT) significantly contributed to
the success of LAMP; his premature, tragic passing has deeply saddened
us. We thank the Dark Cosmology Center for their hospitality during the
Improving Black Hole Masses in Active Galaxies workshop in July 2012,
which provided a venue for conversations that improved this work.
NR 102
TC 155
Z9 155
U1 0
U2 10
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD APR 20
PY 2013
VL 767
IS 2
AR 149
DI 10.1088/0004-637X/767/2/149
PG 27
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 122VR
UT WOS:000317346800052
ER
PT J
AU Heinze, AN
Metchev, S
Apai, D
Flateau, D
Kurtev, R
Marley, M
Radigan, J
Burgasser, AJ
Artigau, E
Plavchan, P
AF Heinze, Aren N.
Metchev, Stanimir
Apai, Daniel
Flateau, Davin
Kurtev, Radostin
Marley, Mark
Radigan, Jacqueline
Burgasser, Adam J.
Artigau, Etienne
Plavchan, Peter
TI WEATHER ON OTHER WORLDS. I. DETECTION OF PERIODIC VARIABILITY IN THE L3
DWARF DENIS-P J1058.7-1548 WITH PRECISE MULTI-WAVELENGTH PHOTOMETRY
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE brown dwarfs; stars: individual (DENIS-P J1058.7-1548); stars: low-mass;
stars: rotation starspots; stars: variables: general; techniques:
photometric
ID EFFECTIVE TEMPERATURE SCALE; TIME-SERIES OBSERVATIONS; BRIGHT ULTRACOOL
DWARFS; SPITZER-SPACE-TELESCOPE; INFRARED ARRAY CAMERA; SKY SURVEY
2MASS; SPECTRAL TYPE-L; LOW-MASS STARS; BROWN DWARF; T-DWARFS
AB Photometric monitoring from warm Spitzer reveals that the L3 dwarf DENIS-P J1058.7-1548 varies sinusoidally in brightness with a period of 4.25(-0.16)(+0.26) hr and an amplitude of 0.388% +/- 0.043% (peak-to-valley) in the 3.6 mu m band, confirming the reality of a 4.31 +/- 0.31 hr periodicity detected in J-band photometry from the SOAR telescope. The J-band variations are a factor of 2.17 +/- 0.35 larger in amplitude than those at 3.6 mu m, while 4.5 mu m Spitzer observations yield a 4.5 mu m/3.6 mu m amplitude ratio of only 0.23 +/- 0.15, consistent with zero 4.5 mu m variability. This wide range in amplitudes indicates rotationally modulated variability due to magnetic phenomena and/or inhomogeneous cloud cover. Weak Ha emission indicates some magnetic activity, but it is difficult to explain the observed amplitudes by magnetic phenomena unless they are combined with cloud inhomogeneities (which might have a magnetic cause). However, inhomogeneous cloud cover alone can explain all our observations, and our data align with theory in requiring that the regions with the thickest clouds also have the lowest effective temperature. Combined with published v sin(i) results, our rotation period yields a 95% confidence lower limit of R-* >= 0.111 R-circle dot, suggesting upper limits of 320 Myr and 0.055 M-circle dot on the age and mass. These limits should be regarded cautiously because of similar to 3 sigma inconsistencies with other data; however, a lower limit of 45 degrees. on the inclination is more secure. DENIS-P J1058.7-1548 is only the first of nearly two dozen low-amplitude variables discovered and analyzed by the Weather on Other Worlds project.
C1 [Heinze, Aren N.; Metchev, Stanimir] SUNY Stony Brook, Dept Phys & Astron, Stony Brook, NY 11794 USA.
[Apai, Daniel; Flateau, Davin] Univ Arizona, Dept Astron, Tucson, AZ 85721 USA.
[Apai, Daniel; Flateau, Davin] Univ Arizona, Dept Planetary Sci, Tucson, AZ 85721 USA.
[Apai, Daniel; Flateau, Davin] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA.
[Kurtev, Radostin] Univ Valparaiso, Fac Ciencias, Dept Fis & Astron, Valparaiso, Chile.
[Marley, Mark] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Radigan, Jacqueline] Univ Toronto, Dept Astron & Astrophys, Toronto, ON M5S 3H4, Canada.
[Burgasser, Adam J.] Univ Calif San Diego, Ctr Astrophys & Space Sci, La Jolla, CA 92093 USA.
[Artigau, Etienne] Univ Montreal, Dept Phys, Montreal, PQ H3C 3J7, Canada.
[Artigau, Etienne] Univ Montreal, Observ Mt Megantic, Montreal, PQ H3C 3J7, Canada.
[Plavchan, Peter] CALTECH, NASA, Exoplanet Sci Inst, Pasadena, CA 91125 USA.
RP Heinze, AN (reprint author), SUNY Stony Brook, Dept Phys & Astron, Stony Brook, NY 11794 USA.
EM aren.heinze@stonybrook.edu; stanimir.metchev@stonybrook.edu
RI Marley, Mark/I-4704-2013;
OI Marley, Mark/0000-0002-5251-2943
FU NASA through the Spitzer Exploration Science Program Weather on Other
Worlds (program) [GO 80179]; ADAP [NNX11AB18G]; Proyecto [DIUV23/2009];
Centro de Astrofisica de Valparaiso; FONDECYT [1130140]; Space Telescope
Science Institute under U.S. Government [NAG W-2166]
FX We thank Didier Saumon for supplying us with files containing the model
spectra of Saumon & Marley (2008), which we have used to construct our
two-phase models of DENIS 1058. This research was supported by NASA
through the Spitzer Exploration Science Program Weather on Other Worlds
(program GO 80179) and ADAP award NNX11AB18G. This research is also
based on observations obtained at the Southern Astrophysical Research
(SOAR) telescope, which is a joint project of the Ministerio da Ciencia,
Tecnologia, e Inovacao (MCTI) da Republica Federativa do Brasil, the U.
S. National Optical Astronomy Observatory (NOAO), the University of
North Carolina at Chapel Hill (UNC), and Michigan State University
(MSU). The SOAR observations reported herein were made under Chilean
program CN2012A-055. Radostin Kurtev acknowledges support from Proyecto
DIUV23/2009, Centro de Astrofisica de Valparaiso, and FONDECYT through
grant 1130140. We thank Nikole Lewis for supplying us with IDL code to
measure the noise pixel parameter of our data, for allowing us to read
the draft version of her paper describing uses of this parameter in IRAC
photometry, and for additional helpful advice. This publication makes
use of the SIMBAD online database, operated at CDS, Strasbourg, France,
and the VizieR online database (see Ochsenbein et al. 2000). This
publication makes use of data products from the Two Micron All Sky
Survey, which is a joint project of the University of Massachusetts and
the Infrared Processing and Analysis Center/ California Institute of
Technology, funded by the National Aeronautics and Space Administration
and the National Science Foundation. We have also made extensive use of
information and code from Press et al. (1992). We have used digitized
images from the Palomar Sky Survey (available from
http://stdatu.stsci.edu/cgi-bin/dss_form), which were produced at the
Space Telescope Science Institute under U.S. Government grant NAG
W-2166. The images of these surveys are based on photographic data
obtained using the Oschin Schmidt Telescope on Palomar Mountain and the
UK Schmidt Telescope.
NR 86
TC 27
Z9 27
U1 1
U2 9
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD APR 20
PY 2013
VL 767
IS 2
AR 173
DI 10.1088/0004-637X/767/2/173
PG 17
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 122VR
UT WOS:000317346800076
ER
PT J
AU Huber, D
Chaplin, WJ
Christensen-Dalsgaard, J
Gilliland, RL
Kjeldsen, H
Buchhave, LA
Fischer, DA
Lissauer, JJ
Rowe, JF
Sanchis-Ojeda, R
Basu, S
Handberg, R
Hekker, S
Howard, AW
Isaacson, H
Karoff, C
Latham, DW
Lund, MN
Lundkvist, M
Marcy, GW
Miglio, A
Aguirre, VS
Stello, D
Arentoft, T
Barclay, T
Bedding, TR
Burke, CJ
Christiansen, JL
Elsworth, YP
Haas, MR
Kawaler, SD
Metcalfe, TS
Mullally, F
Thompson, SE
AF Huber, Daniel
Chaplin, William J.
Christensen-Dalsgaard, Jorgen
Gilliland, Ronald L.
Kjeldsen, Hans
Buchhave, Lars A.
Fischer, Debra A.
Lissauer, Jack J.
Rowe, Jason F.
Sanchis-Ojeda, Roberto
Basu, Sarbani
Handberg, Rasmus
Hekker, Saskia
Howard, Andrew W.
Isaacson, Howard
Karoff, Christoffer
Latham, David W.
Lund, Mikkel N.
Lundkvist, Mia
Marcy, Geoffrey W.
Miglio, Andrea
Aguirre, Victor Silva
Stello, Dennis
Arentoft, Torben
Barclay, Thomas
Bedding, Timothy R.
Burke, Christopher J.
Christiansen, Jessie L.
Elsworth, Yvonne P.
Haas, Michael R.
Kawaler, Steven D.
Metcalfe, Travis S.
Mullally, Fergal
Thompson, Susan E.
TI FUNDAMENTAL PROPERTIES OF KEPLER PLANET-CANDIDATE HOST STARS USING
ASTEROSEISMOLOGY
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE planetary systems; stars: late-type; stars: oscillations; techniques:
photometric; techniques: spectroscopic
ID SOLAR-LIKE OSCILLATIONS; TRANSIT TIMING OBSERVATIONS; 1ST 4 MONTHS;
STELLAR EVOLUTION DATABASE; FINE GUIDANCE SENSOR; MAIN-SEQUENCE STARS;
RED-GIANT STARS; SUN-LIKE STAR; EXTRASOLAR PLANETS; INPUT CATALOG
AB We have used asteroseismology to determine fundamental properties for 66 Kepler planet-candidate host stars, with typical uncertainties of 3% and 7% in radius and mass, respectively. The results include new asteroseismic solutions for four host stars with confirmed planets (Kepler-4, Kepler-14, Kepler-23 and Kepler-25) and increase the total number of Kepler host stars with asteroseismic solutions to 77. A comparison with stellar properties in the planet-candidate catalog by Batalha et al. shows that radii for subgiants and giants obtained from spectroscopic follow-up are systematically too low by up to a factor of 1.5, while the properties for unevolved stars are in good agreement. We furthermore apply asteroseismology to confirm that a large majority of cool main-sequence hosts are indeed dwarfs and not misclassified giants. Using the revised stellar properties, we recalculate the radii for 107 planet candidates in our sample, and comment on candidates for which the radii change from a previously giant-planet/brown-dwarf/stellar regime to a sub-Jupiter size or vice versa. A comparison of stellar densities from asteroseismology with densities derived from transit models in Batalha et al. assuming circular orbits shows significant disagreement for more than half of the sample due to systematics in the modeled impact parameters or due to planet candidates that may be in eccentric orbits. Finally, we investigate tentative correlations between host-star masses and planet-candidate radii, orbital periods, and multiplicity, but caution that these results may be influenced by the small sample size and detection biases.
C1 [Huber, Daniel; Lissauer, Jack J.; Rowe, Jason F.; Barclay, Thomas; Burke, Christopher J.; Christiansen, Jessie L.; Haas, Michael R.; Mullally, Fergal; Thompson, Susan E.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Chaplin, William J.; Miglio, Andrea; Elsworth, Yvonne P.] Univ Birmingham, Sch Phys & Astron, Birmingham B15 2TT, W Midlands, England.
[Chaplin, William J.; Christensen-Dalsgaard, Jorgen; Kjeldsen, Hans; Handberg, Rasmus; Karoff, Christoffer; Lund, Mikkel N.; Lundkvist, Mia; Aguirre, Victor Silva; Stello, Dennis; Arentoft, Torben; Bedding, Timothy R.] Aarhus Univ, Dept Phys & Astron, Stellar Astrophys Ctr, DK-8000 Aarhus C, Denmark.
[Gilliland, Ronald L.] Penn State Univ, Ctr Exoplanets & Habitable Worlds, University Pk, PA 16802 USA.
[Buchhave, Lars A.] Univ Copenhagen, Niels Bohr Inst, DK-2100 Copenhagen, Denmark.
[Buchhave, Lars A.] Univ Copenhagen, Nat Hist Museum Denmark, Ctr Star & Planet Format, DK-1350 Copenhagen, Denmark.
[Fischer, Debra A.; Basu, Sarbani] Yale Univ, Dept Astron, New Haven, CT 06511 USA.
[Sanchis-Ojeda, Roberto] MIT, Dept Phys, Cambridge, MA 02139 USA.
[Hekker, Saskia] Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1098 XH Amsterdam, Netherlands.
[Howard, Andrew W.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA.
[Isaacson, Howard; Marcy, Geoffrey W.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA.
[Latham, David W.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Stello, Dennis; Bedding, Timothy R.] Univ Sydney, Sch Phys, Sydney Inst Astron SIfA, Sydney, NSW 2006, Australia.
[Kawaler, Steven D.] Iowa State Univ, Dept Phys & Astron, Ames, IA 50011 USA.
[Metcalfe, Travis S.] Space Sci Inst, Boulder, CO 80301 USA.
RP Huber, D (reprint author), NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
EM daniel.huber@nasa.gov
RI Howard, Andrew/D-4148-2015;
OI Lund, Mikkel Norup/0000-0001-9214-5642; Lundkvist, Mia
Sloth/0000-0002-8661-2571; Fischer, Debra/0000-0003-2221-0861; Handberg,
Rasmus/0000-0001-8725-4502; Kawaler, Steven/0000-0002-6536-6367; Howard,
Andrew/0000-0001-8638-0320; Bedding, Timothy/0000-0001-5943-1460;
Buchhave, Lars A./0000-0003-1605-5666; Metcalfe,
Travis/0000-0003-4034-0416; Karoff, Christoffer/0000-0003-2009-7965;
Bedding, Tim/0000-0001-5222-4661; Basu, Sarbani/0000-0002-6163-3472
FU NASA's Science Mission Directorate; NSF [AST-1105930]; Netherlands
Organisation for Scientific Research (NWO); NASA [NNX13AE91G]; Danish
National Research Foundation [DNRF106]; ASTERISK project (ASTERoseismic
Investigations with SONG and Kepler); European Research Council [267864]
FX We thank Willie Torres, Josh Winn, and our anonymous referee for helpful
comments and discussions. We furthermore gratefully acknowledge the
entire Kepler team and everyone involved in the Kepler mission for
making this paper possible. Funding for the Kepler mission is provided
by NASA's Science Mission Directorate. D.H. is supported by an
appointment to the NASA Postdoctoral Program at Ames Research Center,
administered by Oak Ridge Associated Universities through a contract
with NASA. S.B. acknowledges NSF grant AST-1105930. S.H. acknowledges
financial support from the Netherlands Organisation for Scientific
Research (NWO). T.S.M. acknowledges NASA grant NNX13AE91G. Funding for
the Stellar Astrophysics Centre is provided by The Danish National
Research Foundation (Grant DNRF106). The research is supported by the
ASTERISK project (ASTERoseismic Investigations with SONG and Kepler)
funded by the European Research Council (Grant agreement No.: 267864).
NR 153
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PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD APR 20
PY 2013
VL 767
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AR 127
DI 10.1088/0004-637X/767/2/127
PG 17
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 122VR
UT WOS:000317346800030
ER
PT J
AU Nissanke, S
Kasliwal, M
Georgieva, A
AF Nissanke, Samaya
Kasliwal, Mansi
Georgieva, Alexandra
TI IDENTIFYING ELUSIVE ELECTROMAGNETIC COUNTERPARTS TO GRAVITATIONAL WAVE
MERGERS: AN END-TO-END SIMULATION
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE binaries: close; catalogs; gamma-ray burst: general; gravitational
waves; stars: neutron; surveys Online-only material: color figures
ID GAMMA-RAY BURSTS; NEUTRON-STAR MERGERS; OBSERVATORY SUPERNOVA SEARCH;
COMPACT OBJECT MERGERS; HOST GALAXY; BINARY INSPIRALS; TRANSIENT EVENTS;
DRIVEN WIND; JET BREAKS; R-PROCESS
AB Combined gravitational wave (GW) and electromagnetic (EM) observations of compact binary mergers should enable detailed studies of astrophysical processes in the strong-field gravity regime. This decade, ground-based GW interferometers promise to routinely detect compact binary mergers. Unfortunately, networks of GW interferometers have poor angular resolution on the sky and their EM signatures are predicted to be faint. Therefore, a challenging goal will be to unambiguously pinpoint the EM counterparts of GW mergers. We perform the first comprehensive end-to-end simulation that focuses on: (1) GW sky localization, distance measures, and volume errors with two compact binary populations and four different GW networks; (2) subsequent EM detectability by a slew of multiwavelength telescopes; and (3) final identification of the merger counterpart amidst a sea of possible astrophysical false positives. First, we find that double neutron star binary mergers can be detected out to a maximum distance of 400 Mpc (or 750 Mpc) by three (or five) detector GW networks, respectively. Neutron-star-black-hole binary mergers can be detected a factor of 1.5 further out; their median to maximum sky localizations are 50-170 deg(2) (or 6-65 deg(2)) for a three (or five) detector GW network. Second, by optimizing depth, cadence, and sky area, we quantify relative fractions of optical counterparts that are detectable by a suite of different aperture-size telescopes across the globe. Third, we present five case studies to illustrate the diversity of scenarios in secure identification of the EM counterpart. We discuss the case of a typical binary, neither beamed nor nearby, and the challenges associated with identifying an EM counterpart at both low and high Galactic latitudes. For the first time, we demonstrate how construction of low-latency GW volumes in conjunction with local universe galaxy catalogs can help solve the problem of false positives. We conclude with strategies that would best prepare us for successfully identifying the elusive EM counterpart of a GW merger.
C1 [Nissanke, Samaya; Georgieva, Alexandra] CALTECH, Pasadena, CA 91125 USA.
[Nissanke, Samaya] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Kasliwal, Mansi] Carnegie Inst Sci, Pasadena, CA 91101 USA.
RP Nissanke, S (reprint author), CALTECH, Pasadena, CA 91125 USA.
FU National Aeronautics and Space Administration
FX We are very grateful to Jean-Michel Desert, Dale Frail, Chris Hirata,
Shri Kulkarni, and Setu Mohta for careful reading of the manuscript. We
thank Ernazar Abdikamalov, Paul Groot, Gregg Hallinan, Brian Metzger,
Sterl Phinney, Tony Piro, Tom Prince, Jon Sievers, and Linqing Wen for
useful discussions. S.M.N. thanks the ITC for hospitality and
discussions there with Edo Berger and Josh Grindlay. We thank Anand
Sengupta and Tarun Souradeep for providing LIGO India's (previously
referred to as IndIGO) position and orientation. We thank Haixing Miao
for providing the anticipated advanced LIGO noise curve with optical
squeezing and Masaki Ando, Larry Price, and Stan Whitcomb for KAGRA and
LIGO follow-up references. We thank Neil Gehrels, David Kaplan, Peter
Nugent, and Fang Yuan for providing specifications of Lobster-ISS, WIYN,
La Silla Quest, and Skymapper, respectively. Some of the simulations
were performed using the Sunnyvale cluster at CITA. Part of this work
was performed at the Jet Propulsion Laboratory, California Institute of
Technology, under contract with the National Aeronautics and Space
Administration. Government sponsorship acknowledged.
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD APR 20
PY 2013
VL 767
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AR 124
DI 10.1088/0004-637X/767/2/124
PG 21
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 122VR
UT WOS:000317346800027
ER
PT J
AU Quintana, EV
Rowe, JF
Barclay, T
Howell, SB
Ciardi, DR
Demory, BO
Caldwell, DA
Borucki, WJ
Christiansen, JL
Jenkins, JM
Klaus, TC
Fulton, BJ
Morris, RL
Sanderfer, DT
Shporer, A
Smith, JC
Still, M
Thompson, SE
AF Quintana, Elisa V.
Rowe, Jason F.
Barclay, Thomas
Howell, Steve B.
Ciardi, David R.
Demory, Brice-Olivier
Caldwell, Douglas A.
Borucki, William J.
Christiansen, Jessie L.
Jenkins, Jon M.
Klaus, Todd C.
Fulton, Benjamin J.
Morris, Robert L.
Sanderfer, Dwight T.
Shporer, Avi
Smith, Jeffrey C.
Still, Martin
Thompson, Susan E.
TI CONFIRMATION OF HOT JUPITER KEPLER-41b VIA PHASE CURVE ANALYSIS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE planetary systems; techniques: photometric
ID EXTRASOLAR GIANT PLANETS; ATMOSPHERIC CHARACTERIZATION; ELLIPSOIDAL
VARIATIONS; SOPHIE VELOCIMETRY; LIGHT CURVES; HIGH ALBEDO; LOW-MASS;
COMPANIONS; PHOTOMETRY; DISCOVERY
AB We present high precision photometry of Kepler-41, a giant planet in a 1.86 day orbit around a G6V star that was recently confirmed through radial velocity measurements. We have developed a new method to confirm giant planets solely from the photometric light curve, and we apply this method herein to Kepler-41 to establish the validity of this technique. We generate a full phase photometric model by including the primary and secondary transits, ellipsoidal variations, Doppler beaming, and reflected/emitted light from the planet. Third light contamination scenarios that can mimic a planetary transit signal are simulated by injecting a full range of dilution values into the model, and we re-fit each diluted light curve model to the light curve. The resulting constraints on the maximum occultation depth and stellar density combined with stellar evolution models rules out stellar blends and provides a measurement of the planet's mass, size, and temperature. We expect about two dozen Kepler giant planets can be confirmed via this method.
C1 [Quintana, Elisa V.; Rowe, Jason F.; Caldwell, Douglas A.; Christiansen, Jessie L.; Jenkins, Jon M.; Morris, Robert L.; Smith, Jeffrey C.; Thompson, Susan E.] SETI Inst, Mountain View, CA 94043 USA.
[Barclay, Thomas] NASA, Ames Res Ctr, Bay Area Environm Res Inst, Moffett Field, CA 94035 USA.
[Howell, Steve B.; Borucki, William J.; Sanderfer, Dwight T.; Still, Martin] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Ciardi, David R.] CALTECH, NASA Exoplanet Sci Inst, Pasadena, CA 91125 USA.
[Demory, Brice-Olivier] MIT, Dept Earth Atmospher & Planetary Sci, Cambridge, MA 02139 USA.
[Klaus, Todd C.] NASA, Ames Res Ctr, Orbital Sci Corp, Moffett Field, CA 94035 USA.
[Fulton, Benjamin J.; Shporer, Avi] Las Cumbres Observ Global Telescope Network, Santa Barbara, CA 93117 USA.
[Fulton, Benjamin J.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA.
[Shporer, Avi] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA.
RP Quintana, EV (reprint author), SETI Inst, 189 Bernardo Ave,Suite 100, Mountain View, CA 94043 USA.
EM elisa.quintana@nasa.gov
RI Caldwell, Douglas/L-7911-2014;
OI Caldwell, Douglas/0000-0003-1963-9616; Ciardi,
David/0000-0002-5741-3047; Demory, Brice-Olivier/0000-0002-9355-5165
FU NASA Science Mission directorate; NASA [NAS5-26555]; NASA Office of
Space Science [NNX09AF08G]
FX This paper includes data collected by the Kepler mission. Funding for
the Kepler mission is provided by the NASA Science Mission directorate.
Some/all of the data presented in this paper were obtained from the
Mikulski Archive for Space Telescopes (MAST). STScI is operated by the
Association of Universities for Research in Astronomy, Inc., under NASA
contract NAS5-26555. Support for MAST for non-HST data is provided by
the NASA Office of Space Science via grant NNX09AF08G and by other
grants and contracts.
NR 45
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PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD APR 20
PY 2013
VL 767
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AR 137
DI 10.1088/0004-637X/767/2/137
PG 9
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 122VR
UT WOS:000317346800040
ER
PT J
AU Titarchuk, L
Seifina, E
Frontera, F
AF Titarchuk, Lev
Seifina, Elena
Frontera, Filippo
TI SPECTRAL STATE EVOLUTION OF 4U 1820-30: THE STABILITY OF THE SPECTRAL
INDEX OF THE COMPTONIZATION TAIL
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE accretion, accretion disks; black hole physics; radiation mechanisms:
non-thermal; stars: individual (4U 1820-30)
ID X-RAY BINARIES; QUASI-PERIODIC OSCILLATIONS; ENERGY CONCENTRATOR
SPECTROMETER; PHOTOSPHERIC RADIUS EXPANSION; BLACK-HOLE BINARIES;
NEUTRON-STAR; ASTRONOMY SATELLITE; TIMING EXPLORER; MXB 1728-34;
XMM-NEWTON
AB We analyze the X-ray spectra and their timing properties of the compact X-ray binary 4U 1820-30. We establish spectral transitions in this source seen with BeppoSAX and the Rossi X-ray Timing Explorer (RXTE). During the RXTE observations (1996-2009), the source was in the soft state approximately similar to 75% of the time making the lower banana and upper banana transitions combined with long-term low-high state transitions. We reveal that all of the X-ray spectra of 4U 1820-30 are fit by a combination of a thermal (Blackbody) component, a Comptonization component (COMPTB), and a Gaussian-line component. Thus, using this spectral analysis, we find that the photon power-law index Gamma of the Comptonization component is almost unchangeable (Gamma similar to 2), while the electron temperature kT(e) changes from 2.9 to 21 keV during these spectral events. We also establish that for these spectral events the normalization of the COMPTB component (which is proportional to the mass accretion rate (M) over dot) increases by a factor of eight when kT(e) decreases from 21 keV to 2.9 keV. Previously, this index stability effect was also found analyzing X-ray data for the Z-source GX 340+0 and for the atolls 4U 1728-34 and GX 3+1. Thus, we can suggest that this spectral stability property is a spectral signature of an accreting neutron star source. On the other hand, in a black hole binary Gamma monotonically increases with (M) over dot and ultimately its value saturates at large (M) over dot.
C1 [Titarchuk, Lev; Frontera, Filippo] Univ Ferrara, Dipartimento Fis, I-44122 Ferrara, Italy.
[Titarchuk, Lev] George Mason Univ, Fairfax, VA 22030 USA.
[Titarchuk, Lev] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20770 USA.
[Seifina, Elena] Moscow MV Lomonosov State Univ, Sternberg Astron Inst, Moscow 119992, Russia.
RP Titarchuk, L (reprint author), Univ Ferrara, Dipartimento Fis, Via Saragat 1, I-44122 Ferrara, Italy.
EM titarchuk@fe.infn.it; seif@sai.msu.ru; frontera@fe.infn.it
NR 64
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PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD APR 20
PY 2013
VL 767
IS 2
AR 160
DI 10.1088/0004-637X/767/2/160
PG 23
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 122VR
UT WOS:000317346800063
ER
PT J
AU Winebarger, A
Tripathi, D
Mason, HE
Del Zanna, G
AF Winebarger, Amy
Tripathi, Durgesh
Mason, Helen E.
Del Zanna, Giulio
TI DOPPLER SHIFTS IN ACTIVE REGION MOSS USING SOHO/SUMER
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE Sun: atmosphere; Sun: corona; Sun: transition region; Sun: UV radiation
ID EUV IMAGING SPECTROMETER; TRANSITION-REGION; CORONAL-EXPLORER; HINODE
EIS; SUMER TELESCOPE; LOOP MODELS; DYNAMICS; FLOWS; RESOLUTION; SPECTRUM
AB The velocity of the plasma at the footpoint of hot loops in active region cores can be used to discriminate between different heating frequencies. Velocities on the order of a few kilometers per second would indicate low-frequency heating on sub-resolution strands, while velocities close to zero would indicate high-frequency (steady) heating. To discriminate between these two values requires accurate velocity measurements; previous velocity measurements suffer from large uncertainties, mainly due to the lack of an absolute wavelength reference scale. In this paper, we determine the velocity in the loop footpoints using observations from Solar Ultraviolet Measurements of Emitted Radiation (SUMER) on Solar and Heliospheric Observatory. We use neutral spectral lines to determine the wavelength scale of the observations with an uncertainty in the absolute velocity of <3.5 km s(-1) and co-aligned Transition Region and Coronal Explorer (TRACE) images to identify footpoint regions. We studied three different active regions and found average redshifts in the Ne VIII 770 angstrom emission line (formed at 6 x 10(5) K) of 5.17 +/- 5.37 km s(-1) and average redshifts in the C IV 1548 and 1550 angstrom emission lines (formed at 1 x 10(5) K) of 13.94 +/- 4.93 km s(-1) and 14.91 +/- 6.09 km s(-1), respectively. We find no correlation between the brightness in the spectral line and the measured velocity, nor do we find correlation between the Ne VIII and C IV velocities measured co-spatially and co-temporally. SUMER scanned two of the active regions twice; in those active regions we find positive correlation between the co-spatial velocities measured during the first and second scans. These results provide definitive and quantitative measurements for comparisons with simulations of different coronal heating mechanisms.
C1 [Winebarger, Amy] NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA.
[Tripathi, Durgesh] Interuniv Ctr Astron & Astrophys, Pune 411007, Maharashtra, India.
[Mason, Helen E.; Del Zanna, Giulio] Univ Cambridge, Dept Appl Math & Theoret Phys, Cambridge CB3 0WA, England.
RP Winebarger, A (reprint author), NASA, George C Marshall Space Flight Ctr, VP 62, Huntsville, AL 35812 USA.
RI Tripathi, Durgesh/D-9390-2012
OI Tripathi, Durgesh/0000-0003-1689-6254
FU NASA SRT program; DST under Fast Track Scheme [SERB/F/3369/2012-2013];
STFC (UK)
FX A.R.W. was supported by the NASA SR&T program for this work. D. T.
acknowledges the support from DST under Fast Track Scheme
(SERB/F/3369/2012-2013). G.D.Z. and H. E. M. acknowledge support from
STFC (UK). SOHO is a mission of international collaboration between ESA
and NASA.
NR 50
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PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD APR 20
PY 2013
VL 767
IS 2
AR 107
DI 10.1088/0004-637X/767/2/107
PG 8
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 122VR
UT WOS:000317346800010
ER
PT J
AU Sonbas, E
MacLachlan, GA
Shenoy, A
Dhuga, KS
Parke, WC
AF Sonbas, E.
MacLachlan, G. A.
Shenoy, A.
Dhuga, K. S.
Parke, W. C.
TI A NEW CORRELATION BETWEEN GRB X-RAY FLARES AND THE PROMPT EMISSION
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE gamma-ray burst: general; methods: data analysis
ID INTERNAL SHOCKS; ENGINE ACTIVITY; LIGHT CURVES; BURSTS; SWIFT;
VARIABILITY; MODEL; LONG; LUMINOSITY; LAG
AB From a sample of gamma-ray bursts (GRBs) detected by the Fermi and Swift missions, we have extracted the minimum variability timescales for temporal structures in the light curves associated with the prompt emission and X-ray flares. A comparison of this variability timescale with pulse parameters such as rise times, determined via pulse-fitting procedures, and spectral lags, extracted via the cross-correlation function, indicates a tight correlation between these temporal features for both the X-ray flares and the prompt emission. These correlations suggest a common origin for the production of X-ray flares and the prompt emission in GRBs.
C1 [Sonbas, E.] Adiyaman Univ, Dept Phys, TR-02040 Adiyaman, Turkey.
[Sonbas, E.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[MacLachlan, G. A.; Shenoy, A.; Dhuga, K. S.; Parke, W. C.] George Washington Univ, Dept Phys, Washington, DC 20052 USA.
RP Sonbas, E (reprint author), Adiyaman Univ, Dept Phys, TR-02040 Adiyaman, Turkey.
EM edasonbas@yahoo.com
FU Swift mission
FX This work made use of data supplied by the UK Swift Science Data Centre
at the University of Leicester. The work of E.S. was partially supported
through the Swift mission (PI: N. Gehrels) and is gratefully
acknowledged.
NR 30
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 2041-8205
J9 ASTROPHYS J LETT
JI Astrophys. J. Lett.
PD APR 20
PY 2013
VL 767
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AR L28
DI 10.1088/2041-8205/767/2/L28
PG 5
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 123SN
UT WOS:000317411100008
ER
PT J
AU Blaber, EA
Dvorochkin, N
Lee, C
Alwood, JS
Yousuf, R
Pianetta, P
Globus, RK
Burns, BP
Almeida, EAC
AF Blaber, Elizabeth A.
Dvorochkin, Natalya
Lee, Chialing
Alwood, Joshua S.
Yousuf, Rukhsana
Pianetta, Piero
Globus, Ruth K.
Burns, Brendan P.
Almeida, Eduardo A. C.
TI Microgravity Induces Pelvic Bone Loss through Osteoclastic Activity,
Osteocytic Osteolysis, and Osteoblastic Cell Cycle Inhibition by
CDKN1a/p21
SO PLOS ONE
LA English
DT Article
ID MATRIX METALLOPROTEINASES MMPS; SKELETAL-MUSCLE; GENE-EXPRESSION;
TRABECULAR BONE; SPACE-FLIGHT; SIMULATED MICROGRAVITY; GROWING RATS;
BED-REST; TGF-BETA; IN-VITRO
AB Bone is a dynamically remodeled tissue that requires gravity-mediated mechanical stimulation for maintenance of mineral content and structure. Homeostasis in bone occurs through a balance in the activities and signaling of osteoclasts, osteoblasts, and osteocytes, as well as proliferation and differentiation of their stem cell progenitors. Microgravity and unloading are known to cause osteoclast-mediated bone resorption; however, we hypothesize that osteocytic osteolysis, and cell cycle arrest during osteogenesis may also contribute to bone loss in space. To test this possibility, we exposed 16-week-old female C57BL/6J mice (n = 8) to microgravity for 15-days on the STS-131 space shuttle mission. Analysis of the pelvis by mu CT shows decreases in bone volume fraction (BV/TV) of 6.29%, and bone thickness of 11.91%. TRAP-positive osteoclast-covered trabecular bone surfaces also increased in microgravity by 170% (p = 0.004), indicating osteoclastic bone degeneration. High-resolution X-ray nanoCT studies revealed signs of lacunar osteolysis, including increases in cross-sectional area (+17%, p = 0.022), perimeter (+14%, p = 0.008), and canalicular diameter (+6%, p = 0.037). Expression of matrix metalloproteinases (MMP) 1, 3, and 10 in bone, as measured by RT-qPCR, was also up-regulated in microgravity (+12.94, +2.98 and +16.85 fold respectively, p<0.01), with MMP10 localized to osteocytes, and consistent with induction of osteocytic osteolysis. Furthermore, expression of CDKN1a/p21 in bone increased 3.31 fold (p<0.01), and was localized to osteoblasts, possibly inhibiting the cell cycle during tissue regeneration as well as conferring apoptosis resistance to these cells. Finally the apoptosis inducer Trp53 was down-regulated by -1.54 fold (p<0.01), possibly associated with the quiescent survival-promoting function of CDKN1a/p21. In conclusion, our findings identify the pelvic and femoral region of the mouse skeleton as an active site of rapid bone loss in microgravity, and indicate that this loss is not limited to osteoclastic degradation. Therefore, this study offers new evidence for microgravity-induced osteocytic osteolysis, and CDKN1a/p21-mediated osteogenic cell cycle arrest.
C1 [Blaber, Elizabeth A.; Dvorochkin, Natalya; Lee, Chialing; Alwood, Joshua S.; Yousuf, Rukhsana; Globus, Ruth K.; Almeida, Eduardo A. C.] NASA, Ames Res Ctr, Space Biosci Div, Moffett Field, CA 94035 USA.
[Blaber, Elizabeth A.; Burns, Brendan P.] Univ New S Wales, Sch Biotechnol & Biomol Sci, Sydney, NSW, Australia.
[Pianetta, Piero] SLAC Natl Accelerator Lab, Stanford Synchrotron Radiat Lightsource, Menlo Pk, CA USA.
RP Almeida, EAC (reprint author), NASA, Ames Res Ctr, Space Biosci Div, Moffett Field, CA 94035 USA.
EM e.almeida@nasa.gov
OI BURNS, BRENDAN/0000-0002-2962-2597
FU [NASA-NNH08ZTT003]
FX This work was supported by NASA-NNH08ZTT003. The funders had no role in
study design, data collection and analysis, decision to publish, or
preparation of the manuscript.
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U2 36
PU PUBLIC LIBRARY SCIENCE
PI SAN FRANCISCO
PA 1160 BATTERY STREET, STE 100, SAN FRANCISCO, CA 94111 USA
SN 1932-6203
J9 PLOS ONE
JI PLoS One
PD APR 18
PY 2013
VL 8
IS 4
AR e61372
DI 10.1371/journal.pone.0061372
PG 15
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 130IU
UT WOS:000317908700027
PM 23637819
ER
PT J
AU Riechers, DA
Bradford, CM
Clements, DL
Dowell, CD
Perez-Fournon, I
Ivison, RJ
Bridge, C
Conley, A
Fu, H
Vieira, JD
Wardlow, J
Calanog, J
Cooray, A
Hurley, P
Neri, R
Kamenetzky, J
Aguirre, JE
Altieri, B
Arumugam, V
Benford, DJ
Bethermin, M
Bock, J
Burgarella, D
Cabrera-Lavers, A
Chapman, SC
Cox, P
Dunlop, JS
Earle, L
Farrah, D
Ferrero, P
Franceschini, A
Gavazzi, R
Glenn, J
Solares, EAG
Gurwell, MA
Halpern, M
Hatziminaoglou, E
Hyde, A
Ibar, E
Kovacs, A
Krips, M
Lupu, RE
Maloney, PR
Martinez-Navajas, P
Matsuhara, H
Murphy, EJ
Naylor, BJ
Nguyen, HT
Oliver, SJ
Omont, A
Page, MJ
Petitpas, G
Rangwala, N
Roseboom, IG
Scott, D
Smith, AJ
Staguhn, JG
Streblyanska, A
Thomson, AP
Valtchanov, I
Viero, M
Wang, L
Zemcov, M
Zmuidzinas, J
AF Riechers, Dominik A.
Bradford, C. M.
Clements, D. L.
Dowell, C. D.
Perez-Fournon, I.
Ivison, R. J.
Bridge, C.
Conley, A.
Fu, Hai
Vieira, J. D.
Wardlow, J.
Calanog, J.
Cooray, A.
Hurley, P.
Neri, R.
Kamenetzky, J.
Aguirre, J. E.
Altieri, B.
Arumugam, V.
Benford, D. J.
Bethermin, M.
Bock, J.
Burgarella, D.
Cabrera-Lavers, A.
Chapman, S. C.
Cox, P.
Dunlop, J. S.
Earle, L.
Farrah, D.
Ferrero, P.
Franceschini, A.
Gavazzi, R.
Glenn, J.
Solares, E. A. Gonzalez
Gurwell, M. A.
Halpern, M.
Hatziminaoglou, E.
Hyde, A.
Ibar, E.
Kovacs, A.
Krips, M.
Lupu, R. E.
Maloney, P. R.
Martinez-Navajas, P.
Matsuhara, H.
Murphy, E. J.
Naylor, B. J.
Nguyen, H. T.
Oliver, S. J.
Omont, A.
Page, M. J.
Petitpas, G.
Rangwala, N.
Roseboom, I. G.
Scott, D.
Smith, A. J.
Staguhn, J. G.
Streblyanska, A.
Thomson, A. P.
Valtchanov, I.
Viero, M.
Wang, L.
Zemcov, M.
Zmuidzinas, J.
TI A dust-obscured massive maximum-starburst galaxy at a redshift of 6.34
SO NATURE
LA English
DT Article
ID STAR-FORMING GALAXIES; SIMILAR-TO 6; MOLECULAR GAS; SUBMILLIMETER
GALAXIES; EARLY UNIVERSE; HOST GALAXY; QUASARS; DISKS; FIELD
AB Massive present-day early-type (elliptical and lenticular) galaxies probably gained the bulk of their stellar mass and heavy elements through intense, dust-enshrouded starbursts-that is, increased rates of star formation-in the most massive dark-matter haloes at early epochs. However, it remains unknown how soon after the Big Bang massive starburst progenitors exist. The measured redshift (z) distribution of dusty, massive starbursts has long been suspected to be biased low in z owing to selection effects(1), as confirmed by recent findings of systems with redshifts as high as similar to 5 (refs 2-4). Here we report the identification of a massive starburst galaxy at z = 6.34 through a submillimetre colour-selection technique. We unambiguously determined the redshift from a suite of molecular and atomic fine-structure cooling lines. These measurements reveal a hundred billion solar masses of highly excited, chemically evolved interstellar medium in this galaxy, which constitutes at least 40 per cent of the baryonic mass. A 'maximum starburst' converts the gas into stars at a rate more than 2,000 times that of the Milky Way, a rate among the highest observed at any epoch. Despite the overall downturn in cosmic star formation towards the highest redshifts(5), it seems that environments mature enough to form the most massive, intense starbursts existed at least as early as 880 million years after the Big Bang.
C1 [Riechers, Dominik A.; Bradford, C. M.; Dowell, C. D.; Bridge, C.; Vieira, J. D.; Cooray, A.; Bock, J.; Kovacs, A.; Murphy, E. J.; Nguyen, H. T.; Viero, M.; Zemcov, M.; Zmuidzinas, J.] CALTECH, Pasadena, CA 91125 USA.
[Riechers, Dominik A.] Cornell Univ, Ithaca, NY 14853 USA.
[Bradford, C. M.; Dowell, C. D.; Bock, J.; Naylor, B. J.; Nguyen, H. T.; Zemcov, M.; Zmuidzinas, J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Clements, D. L.; Hyde, A.] Univ London Imperial Coll Sci Technol & Med, Blackett Lab, Astrophys Grp, London SW7 2AZ, England.
[Perez-Fournon, I.; Cabrera-Lavers, A.; Ferrero, P.; Martinez-Navajas, P.; Streblyanska, A.] Inst Astrofis Canarias, E-38200 Tenerife, Spain.
[Perez-Fournon, I.; Cabrera-Lavers, A.; Ferrero, P.; Martinez-Navajas, P.; Streblyanska, A.] Univ La Laguna, Dept Astrofis, E-38205 Tenerife, Spain.
[Ivison, R. J.; Ibar, E.] Royal Observ, UK Astron Technol Ctr, Edinburgh EH9 3HJ, Midlothian, Scotland.
[Ivison, R. J.; Arumugam, V.; Dunlop, J. S.; Roseboom, I. G.; Thomson, A. P.] Univ Edinburgh, Royal Observ, Inst Astron, Edinburgh EH9 3HJ, Midlothian, Scotland.
[Conley, A.; Earle, L.; Glenn, J.; Maloney, P. R.] Univ Colorado, Ctr Astrophys & Space Astron UCB 389, Boulder, CO 80309 USA.
[Fu, Hai; Wardlow, J.; Calanog, J.; Cooray, A.] Univ Calif Irvine, Dept Phys & Astron, Irvine, CA 92697 USA.
[Hurley, P.; Oliver, S. J.; Roseboom, I. G.; Smith, A. J.; Wang, L.] Univ Sussex, Dept Phys & Astron, Ctr Astron, Brighton BN1 9QH, E Sussex, England.
[Neri, R.; Cox, P.; Krips, M.] Inst Radio Astron Millimetr, F-38406 St Martin Dheres, France.
[Kamenetzky, J.; Glenn, J.; Rangwala, N.] Univ Colorado, Dept Astrophys & Planetary Sci, CASA UCB 389, Boulder, CO 80309 USA.
[Aguirre, J. E.; Lupu, R. E.] Univ Penn, Dept Phys & Astron, Philadelphia, PA 19104 USA.
[Altieri, B.; Valtchanov, I.] European Space Astron Ctr, Herschel Sci Ctr, Madrid 28691, Spain.
[Benford, D. J.; Staguhn, J. G.] NASA, Observat Cosmol Lab, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Bethermin, M.] Univ Paris Diderot, CEA Saclay, Lab AIM Paris Saclay, CEA,DSM,Irfu,CNRS, F-91191 Gif Sur Yvette, France.
[Bethermin, M.] Univ Paris 11, IAS, F-91405 Orsay, France.
[Bethermin, M.] CNRS, UMR 8617, F-91405 Orsay, France.
[Burgarella, D.] Aix Marseille Univ, CNRS, Lab Astrophys Marseille, UMR7326, F-13388 Marseille, France.
[Cabrera-Lavers, A.] Grantecan SA, Ctr Astrofis La Palma, E-38712 Brena Baja, La Palma, Spain.
[Chapman, S. C.; Solares, E. A. Gonzalez] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England.
[Farrah, D.] Virginia Tech, Dept Phys, Blacksburg, VA 24061 USA.
[Franceschini, A.] Univ Padua, Dipartimento Fis & Astron, I-35122 Padua, Italy.
[Gavazzi, R.; Omont, A.] Univ Paris 06, CNRS, Inst Astrophys Paris, UMR 7095, F-75014 Paris, France.
[Gurwell, M. A.; Petitpas, G.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Halpern, M.; Scott, D.] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada.
[Hatziminaoglou, E.] ESO, D-85748 Garching, Germany.
[Kovacs, A.] Univ Minnesota, Inst Astrophys, Minneapolis, MN 55455 USA.
[Matsuhara, H.] Japan Aerosp & Explorat Agcy, Inst Space & Astronaut Sci, Sagamihara, Kanagawa 2298510, Japan.
[Murphy, E. J.] CALTECH, Infrared Proc & Anal Ctr, Pasadena, CA 91125 USA.
[Page, M. J.] Univ Coll London, Mullard Space Sci Lab, Dorking RH5 6NT, Surrey, England.
[Staguhn, J. G.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA.
RP Riechers, DA (reprint author), CALTECH, 1200 East Calif Blvd,MC 249-17, Pasadena, CA 91125 USA.
EM dr@astro.cornell.edu
RI sebastianovitsch, stepan/G-8507-2013; Lupu, Roxana/P-9060-2014; Wardlow,
Julie/C-9903-2015; Kovacs, Attila/C-1171-2010; Ivison, R./G-4450-2011;
Benford, Dominic/D-4760-2012;
OI Lupu, Roxana/0000-0003-3444-5908; Wardlow, Julie/0000-0003-2376-8971;
Kovacs, Attila/0000-0001-8991-9088; Ivison, R./0000-0001-5118-1313;
Benford, Dominic/0000-0002-9884-4206; Scott,
Douglas/0000-0002-6878-9840; Bethermin, Matthieu/0000-0002-3915-2015;
Altieri, Bruno/0000-0003-3936-0284
NR 30
TC 160
Z9 160
U1 1
U2 30
PU NATURE PUBLISHING GROUP
PI LONDON
PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND
SN 0028-0836
J9 NATURE
JI Nature
PD APR 18
PY 2013
VL 496
IS 7445
BP 329
EP 333
DI 10.1038/nature12050
PG 5
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 126FV
UT WOS:000317599200030
PM 23598341
ER
PT J
AU Su, H
Jiang, JH
Zhai, CX
Perun, VS
Shen, JT
Del Genio, A
Nazarenko, LS
Donner, LJ
Horowitz, L
Seman, C
Morcrette, C
Petch, J
Ringer, M
Cole, J
von Salzen, K
Mesquita, MDS
Iversen, T
Kristjansson, JE
Gettelman, A
Rotstayn, L
Jeffrey, S
Dufresne, JL
Watanabe, M
Kawai, H
Koshiro, T
Wu, TW
Volodin, EM
L'Ecuyer, T
Teixeira, J
Stephens, GL
AF Su, Hui
Jiang, Jonathan H.
Zhai, Chengxing
Perun, Vince S.
Shen, Janice T.
Del Genio, Anthony
Nazarenko, Larissa S.
Donner, Leo J.
Horowitz, Larry
Seman, Charles
Morcrette, Cyril
Petch, Jon
Ringer, Mark
Cole, Jason
von Salzen, Knut
Mesquita, Michel D. S.
Iversen, Trond
Kristjansson, Jon Egill
Gettelman, Andrew
Rotstayn, Leon
Jeffrey, Stephen
Dufresne, Jean-Louis
Watanabe, Masahiro
Kawai, Hideaki
Koshiro, Tsuyoshi
Wu, Tongwen
Volodin, Evgeny M.
L'Ecuyer, Tristan
Teixeira, Joao
Stephens, Graeme L.
TI Diagnosis of regime-dependent cloud simulation errors in CMIP5 models
using "A-Train" satellite observations and reanalysis data
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
DE Clouds; Climate Model; Satellite Observation; CMIP5; A-Train;
large-scale regimes; conditional sampling; model error diagnosis
ID GENERAL-CIRCULATION MODEL; GLOBAL CLIMATE MODEL; ATMOSPHERE;
VARIABILITY; SENSITIVITY; TROPOSPHERE; CONVECTION; MASS
AB The vertical distributions of cloud water content (CWC) and cloud fraction (CF) over the tropical oceans, produced by 13 coupled atmosphere-ocean models submitted to the Phase 5 of Coupled Model Intercomparison Project (CMIP5), are evaluated against CloudSat/CALIPSO observations as a function of large-scale parameters. Available CALIPSO simulator CF outputs are also examined. A diagnostic framework is developed to decompose the cloud simulation errors into large-scale errors, cloud parameterization errors and covariation errors. We find that the cloud parameterization errors contribute predominantly to the total errors for all models. The errors associated with large-scale temperature and moisture structures are relatively greater than those associated with large-scale midtropospheric vertical velocity and lower-level divergence. All models capture the separation of deep and shallow clouds in distinct large-scale regimes; however, the vertical structures of high/low clouds and their variations with large-scale parameters differ significantly from the observations. The CWCs associated with deep convective clouds simulated in most models do not reach as high in altitude as observed, and their magnitudes are generally weaker than CloudSat total CWC, which includes the contribution of precipitating condensates, but are close to CloudSat nonprecipitating CWC. All models reproduce maximum CF associated with convective detrainment, but CALIPSO simulator CFs generally agree better with CloudSat/CALIPSO combined retrieval than the model CFs, especially in the midtroposphere. Model simulated low clouds tend to have little variation with large-scale parameters except lower-troposphere stability, while the observed low cloud CWC, CF, and cloud top height vary consistently in all large-scale regimes.
C1 [Su, Hui; Jiang, Jonathan H.; Zhai, Chengxing; Perun, Vince S.; Shen, Janice T.; Teixeira, Joao; Stephens, Graeme L.] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
[Del Genio, Anthony; Nazarenko, Larissa S.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
[Donner, Leo J.; Horowitz, Larry; Seman, Charles] Geophys Fluid Dynam Lab, Princeton, NJ USA.
[Morcrette, Cyril; Petch, Jon] UK Met Off, Exeter, Devon, England.
[Ringer, Mark] UK Met Off Hadley Ctr MOHC, Exeter, Devon, England.
[Cole, Jason; von Salzen, Knut] Environm Canada, CCCMA, Victoria, BC, Canada.
[Mesquita, Michel D. S.] Uni Res, BCCR, Bergen, Norway.
[Iversen, Trond] NCC, Meteorologisk Inst, Oslo, Norway.
[Kristjansson, Jon Egill] Univ Oslo, Oslo, Norway.
[Gettelman, Andrew] Natl Ctr Atmospher Res, Boulder, CO 80307 USA.
[Rotstayn, Leon] CSIRO, Aspendale, Vic, Australia.
[Watanabe, Masahiro] Univ Tokyo, Atmospher & Ocean Res Inst, Model Interdisciplinary Res Climate MIROC, Chiba, Japan.
[Kawai, Hideaki; Koshiro, Tsuyoshi] Japan Meteorol Agcy, MRI, Tsukuba, Ibaraki, Japan.
[Wu, Tongwen] China Meteorol Adm, BCC, Beijing, Peoples R China.
[Volodin, Evgeny M.] Russian Acad Sci, Inst Numer Math, Moscow, Russia.
[L'Ecuyer, Tristan] Univ Wisconsin, Madison, WI USA.
RP Su, H (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
EM Hui.Su@jpl.nasa.gov
RI L'Ecuyer, Tristan/C-7040-2013; Rotstayn, Leon/A-1756-2012; Horowitz,
Larry/D-8048-2014; Morcrette, Cyril/H-7282-2012; L'Ecuyer,
Tristan/E-5607-2012; Dufresne, Jean-Louis/I-5616-2015; Ringer,
Mark/E-7294-2013; Mesquita, Michel d. S./C-3414-2009; Koshiro,
Tsuyoshi/O-7183-2016
OI Cole, Jason/0000-0003-0450-2748; Rotstayn, Leon/0000-0002-2385-4223;
Horowitz, Larry/0000-0002-5886-3314; Morcrette,
Cyril/0000-0002-4240-8472; L'Ecuyer, Tristan/0000-0002-7584-4836;
Dufresne, Jean-Louis/0000-0003-4764-9600; Ringer,
Mark/0000-0003-4014-2583; Mesquita, Michel d. S./0000-0002-4556-5414;
Koshiro, Tsuyoshi/0000-0003-2971-7446
FU NASA ROSES COUND; AST; NEWS
FX We thank the funding support from NASA ROSES COUND, AST, and NEWS, the
CloudSat/CALIPSO mission teams and relevant satellite mission projects.
We acknowledge PCMDI for archiving CMIP5 model simulations and the ECMWF
Data Server for ECMWF Interim Reanalysis data. This work was carried out
at the Jet Propulsion Laboratory, California Institute of Technology,
under contract with NASA.
NR 56
TC 37
Z9 37
U1 1
U2 45
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-897X
J9 J GEOPHYS RES-ATMOS
JI J. Geophys. Res.-Atmos.
PD APR 16
PY 2013
VL 118
IS 7
BP 2762
EP 2780
DI 10.1029/2012JD018575
PG 19
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 153QT
UT WOS:000319618300006
ER
PT J
AU Xiang, B
Miller, SM
Kort, EA
Santoni, GW
Daube, BC
Commane, R
Angevine, WM
Ryerson, TB
Trainer, MK
Andrews, AE
Nehrkorn, T
Tian, HQ
Wofsy, SC
AF Xiang, Bin
Miller, Scot M.
Kort, Eric A.
Santoni, Gregory W.
Daube, Bruce C.
Commane, Roisin
Angevine, Wayne M.
Ryerson, Tom B.
Trainer, Michael K.
Andrews, Arlyn E.
Nehrkorn, Thomas
Tian, Hanqin
Wofsy, Steven C.
TI Nitrous oxide (N2O) emissions from California based on 2010 CalNex
airborne measurements
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
DE nitrous oxide; emissions; California; fertilizer
ID SPATIAL VARIABILITY; NORTH-AMERICA; STILT MODEL; WATER; SOIL;
ECOSYSTEMS; METHANE; FIELD
AB Nitrous oxide (N2O) is an important gas for climate and for stratospheric chemistry, with a lifetime exceeding 100years. Global concentrations have increased steadily since the 18th century, apparently due to human-associated emissions, principally from the application of nitrogen fertilizers. However, quantitative studies of agricultural emissions at large spatial scales are lacking, inhibited by the difficulty of measuring small enhancements in atmospheric concentration. Here we derive regional emission rates for N2O in the agricultural heartland of California based on analysis of in-situ airborne atmospheric observations collected using a new quantum cascade laser spectrometer. The data were obtained on board the NOAA WP-3 research aircraft during the CalNex (California Research at the Nexus of Air Quality and Climate Change) program in late spring 2010. We coupled the WRF (weather research and forecasting) model, a meso-scale meteorology model, with the STILT (stochastic time-inverted Lagrangian transport) model, a Lagrangian particle dispersion model, to link our in-situ airborne observations to surface emissions. We then used a variety of statistical methods to identify source areas and to optimize emission rates. Our results are consistent with the view that fertilizer application is the largest source of N2O in the Central Valley. The spatial distribution of surface emissions, based on California land use and activity maps, was very different than indicated in the leading emission inventory (EDGAR 4.0). Our estimated total emission flux of N2O for California in May and June was 3 - 4 times larger than the annual mean given for the state by EDGAR and other inventories, indicating a strong seasonal variation. We estimated the statewide total annual emissions of N2O to be 0.042 +/- 0.011 Tg N/year, roughly equivalent to inventory values if we account for seasonal variations using observations obtained in the midwestern United States. This state total N2O emission is 20.5 Tg CO2 equivalent (100year global warming potential=310 CO2 eq/g N2O), accounting for approximately 4% of the state total greenhouse gas emissions.
C1 [Xiang, Bin; Miller, Scot M.; Santoni, Gregory W.; Daube, Bruce C.; Commane, Roisin; Wofsy, Steven C.] Harvard Univ, Sch Engn & Appl Sci, Cambridge, MA 02138 USA.
[Xiang, Bin; Miller, Scot M.; Santoni, Gregory W.; Daube, Bruce C.; Commane, Roisin; Wofsy, Steven C.] Harvard Univ, Dept Earth & Planetary Sci, Cambridge, MA 02138 USA.
[Kort, Eric A.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Angevine, Wayne M.; Ryerson, Tom B.; Trainer, Michael K.; Andrews, Arlyn E.] NOAA, Boulder, CO USA.
[Nehrkorn, Thomas] Atmospher & Environm Res Inc, Lexington, MA USA.
[Tian, Hanqin] Auburn Univ, Sch Forestry & Wildlife Sci, Auburn, AL 36849 USA.
RP Xiang, B (reprint author), Harvard Univ, Sch Engn & Appl Sci, 20 Oxford St, Cambridge, MA 02138 USA.
EM bxiang@seas.harvard.edu
RI Xiang, Bin/E-8034-2012; Commane, Roisin/E-4835-2016; Manager, CSD
Publications/B-2789-2015; Andrews, Arlyn/K-3427-2012; Angevine,
Wayne/H-9849-2013; Trainer, Michael/H-5168-2013; Ryerson,
Tom/C-9611-2009; Tian, Hanqin/A-6484-2012; Kort, Eric/F-9942-2012;
Xiang, Bin/M-2812-2013
OI Nehrkorn, Thomas/0000-0003-0637-3468; Commane,
Roisin/0000-0003-1373-1550; Angevine, Wayne/0000-0002-8021-7116; Tian,
Hanqin/0000-0002-1806-4091; Kort, Eric/0000-0003-4940-7541;
FU NASA [NNX09AJ94G, NNX11AG47G, NNX09AU40G]; NSF [ATM-083091-2]; NOAA
[NA09OAR4310122, NA11OAR4310158]
FX This study was supported by the following grants to Harvard University:
NASA NNX09AJ94G, NNX11AG47G, and NNX09AU40G; NSF ATM-083091-2; and NOAA
NA09OAR4310122 and NA11OAR4310158. We are grateful to the flight crew of
the NOAA P-3 for safely executing a difficult flight mission. B. X.
thanks Jasna Pittman for helpful comments on the manuscript. E.A.K.
thanks the W. M. Keck Institute for Space Studies for support. Portions
of this work were performed at the Jet Propulsion Laboratory, California
Institute of Technology, under contract with NASA.
NR 38
TC 6
Z9 6
U1 2
U2 42
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-897X
J9 J GEOPHYS RES-ATMOS
JI J. Geophys. Res.-Atmos.
PD APR 16
PY 2013
VL 118
IS 7
BP 2809
EP 2820
DI 10.1002/jgrd.50189
PG 12
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 153QT
UT WOS:000319618300009
ER
PT J
AU Dessler, AE
Loeb, NG
AF Dessler, A. E.
Loeb, N. G.
TI Impact of dataset choice on calculations of the short-term cloud
feedback
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
DE cloud feedback; energy budget
ID CLIMATE FEEDBACKS; MODELS; SYSTEM
AB Dessler [2010, hereafter D10] estimated the magnitude of the cloud feedback in response to short-term climate variations and concluded that it was likely positive, with an average magnitude of +0.50 +/- 0.75W/m2/K. This paper investigates the sensitivity of D10's results to the choice of clear-sky top-of-atmosphere flux (Rclear-sky), surface temperature (Ts), and reanalysis data sets. Most of the alternative Rclear-sky data sets produce cloud feedbacks that are close to D10, differing by 0.2-0.3W/m2/K. An exception is the Terra SSF1deg Rclear-sky product, which produces an overall negative cloud feedback. However, a critical examination of those data leads us to conclude that that result is due to problems in the Terra Rclear-sky arising from issues with cloud clearing prior to July 2001. Eliminating the problematic early portion yields a cloud feedback in good agreement with D10. We also present an alternative calculation of the cloud feedback that does not require an estimate of Rclear-sky, and this calculation also produces a positive cloud feedback in agreement with D10. The various Ts data sets produce cloud feedbacks that differ by as much as 0.8W/m2/K. The choice of reanalysis, used as a source of Rclear-sky or as adjustments for the cloud radiative forcing, has a small impact on the inferred cloud feedback. Overall, these results confirm the robustness of D10's estimate of a likely positive feedback.
C1 [Dessler, A. E.] Texas A&M Univ, Dept Atmospher Sci, College Stn, TX 77843 USA.
[Loeb, N. G.] NASA, Langley Res Ctr, Hampton, VA 23665 USA.
RP Dessler, AE (reprint author), Texas A&M Univ, Dept Atmospher Sci, College Stn, TX 77843 USA.
EM adessler@tamu.edu
RI Dessler, Andrew/G-8852-2012
OI Dessler, Andrew/0000-0003-3939-4820
FU NSF [AGS-1012665]
FX This work was supported by NSF grant AGS-1012665 to Texas A&M
University. We thank Mark Zelinka and Troy Masters for their comments on
this paper.
NR 18
TC 6
Z9 6
U1 1
U2 7
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-897X
J9 J GEOPHYS RES-ATMOS
JI J. Geophys. Res.-Atmos.
PD APR 16
PY 2013
VL 118
IS 7
BP 2821
EP 2826
DI 10.1002/jgrd.50199
PG 6
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 153QT
UT WOS:000319618300010
ER
PT J
AU Meyer, TC
Lang, TJ
Rutledge, SA
Lyons, WA
Cummer, SA
Lu, GP
Lindsey, DT
AF Meyer, Tiffany C.
Lang, Timothy J.
Rutledge, Steven A.
Lyons, Walter A.
Cummer, Steven A.
Lu, Gaopeng
Lindsey, Daniel T.
TI Radar and lightning analyses of gigantic jet-producing storms
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
DE Lightning; Gigantic Jet; Thunderstorm
ID BLUE JETS; ELECTRICAL DISCHARGES; TORNADIC STORM; THUNDERSTORMS;
REFLECTIVITY; THUNDERCLOUD; IONOSPHERE; EVOLUTION; STARTERS; VELOCITY
AB An analysis of thunderstorm environment, structure, and evolution associated with six gigantic jets (five negative polarity, one positive) was conducted. Three of these gigantic jets were observed within detection range of very high frequency lightning mapping networks. All six were within range of operational radars and two-dimensional lightning network coverage: five within the National Lightning Detection Network and one within the Global Lightning Detection (GLD360) network. Most of the storms producing the jets formed in moist tropical or tropical-like environments (precipitable water ranged from 37 to 62 kg m-2, and 0-6 km shear from 3.5 to 24.8 m s-1), featuring high convective available potential energy (1200-3500 J kg-1) and low lifted indices (-2.8 to -6.4). The storms had maximum radar reflectivity factors of 54 to 62 dBZ, and 10 dBZ echo contours reached 14-17 km. Storms covered by three-dimensional lightning mappers were near peak altitude of lightning activity (modes of the vertical distributions of radio sources were at altitudes colder than -50 degrees C) and vertical reflectivity intensity, with overshooting echo tops around the times of their jets. Two of the other three jet-producing storms produced their jet around the time of a convective surge as indicated by radar data and likely featured overshooting tops. The observations suggest a link between convective surges, overshooting tops, and the occurrence of gigantic jets, similar to prior modeling studies.
C1 [Meyer, Tiffany C.; Lang, Timothy J.; Rutledge, Steven A.] Colorado State Univ, Dept Atmospher Sci, Ft Collins, CO 80523 USA.
[Meyer, Tiffany C.] Natl Weather Serv, Warning Decis Training Branch, Norman, OK USA.
[Lang, Timothy J.] NASA, Marshall Space Flight Ctr ZP11, Huntsville, AL 35812 USA.
[Lyons, Walter A.] FMA Res Inc, Ft Collins, CO USA.
[Cummer, Steven A.; Lu, Gaopeng] Duke Univ, Elect & Comp Engn Dept, Durham, NC USA.
[Lindsey, Daniel T.] NOAA, NESDIS, STAR, RAMMB, Ft Collins, CO USA.
RP Lang, TJ (reprint author), NASA, Marshall Space Flight Ctr ZP11, Huntsville, AL 35812 USA.
EM tjlangco@gmail.com
RI Lu, Gaopeng/D-9011-2012; Cummer, Steven/A-6118-2008; Lindsey,
Dan/F-5607-2010;
OI Cummer, Steven/0000-0002-0002-0613; Lindsey, Dan/0000-0002-0967-5683;
Lang, Timothy/0000-0003-1576-572X
FU DARPA Nimbus program
FX This work was supported by the DARPA Nimbus program. The authors thank
Vaisala, Inc. for providing the NLDN and GLD360 data used in this study.
Without the observations of the gigantic jets, this study would not have
been possible. The Florida, Oklahoma, and Puerto Rico gigantic jets were
observed by Joel Gonzalez in Florida, by Kevin Palivec in Texas, and by
Frankie Lucena in Puerto Rico, respectively. The authors thank the
editors and reviewers of this manuscript for their assistance in
improving it.
NR 52
TC 7
Z9 7
U1 0
U2 12
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-897X
J9 J GEOPHYS RES-ATMOS
JI J. Geophys. Res.-Atmos.
PD APR 16
PY 2013
VL 118
IS 7
BP 2872
EP 2888
DI 10.1002/jgrd.50302
PG 17
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 153QT
UT WOS:000319618300015
ER
PT J
AU Tesche, M
Wandinger, U
Ansmann, A
Althausen, D
Muller, D
Omar, AH
AF Tesche, M.
Wandinger, U.
Ansmann, A.
Althausen, D.
Mueller, D.
Omar, A. H.
TI Ground-based validation of CALIPSO observations of dust and smoke in the
Cape Verde region
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
DE CALIPSO; SAMUM; lidar; mineral dust; remote sensing; validation
ID AEROSOL OPTICAL DEPTH; SPECTRAL-RESOLUTION LIDAR; NORTH-AFRICAN DUST;
SAHARAN DUST; AERONET MEASUREMENTS; RAMAN LIDAR; MODIS-AQUA; EXTINCTION;
TRANSPORT; PROFILES
AB Ground-based Raman lidar measurements during the second Saharan Mineral Dust Experiment (SAMUM-2) in 2008 were used for validation of measurements of the lidar aboard the Cloud-Aerosol Lidar and Infrared Pathfinder Satellite Observations (CALIPSO) satellite within the dusty environment of the Cape Verde region. SAMUM-2 featured two one-month campaigns in January/February and May/June 2008 to cover different modes of aerosol transport to the tropical Atlantic: dust from northern Africa and biomass-burning smoke from western Africa during winter, and pure Saharan dust during summer. During the investigated time period, 33 CALIPSO overflights occurred at a distance of less than 500 km from the location of the ground-based lidar. Fifteen out of these 33 cases were found suitable for comparing the findings of the two instruments. The parameters for this comparison are the particle backscatter coefficient at 532 and 1064 nm, the extinction coefficient, the lidar ratio (aerosol type), and the particle depolarization ratio at 532 nm, as well as the backscatter-related angstrom ngstrom exponent for the wavelength pair 532/1064 nm. Best agreement was found for the 532 nm backscatter coefficient, while the 532 nm extinction coefficient is underestimated by up to 30%. The latter is due to the use of an effective dust lidar ratio that gives reliable backscatter coefficients but is not suitable to transform these to extinction coefficients. CALIPSO particle depolarization ratios provided in the current (version 3.01) aerosol profile product were found to be affected by a computing error and should be calculated from the perpendicular and total particle backscatter coefficients provided in the same data file. CALIPSO aerosol classification was found to be mostly correct but a demand for homogeneous aerosol layers could improve the retrieval. Suggestions for the improvement of the CALIPSO retrieval by introducing iterative procedures are provided.
C1 [Tesche, M.] Stockholm Univ, Dept Appl Environm Sci ITM, SE-11418 Stockholm, Sweden.
[Wandinger, U.; Ansmann, A.; Althausen, D.; Mueller, D.] Leibniz Inst Tropospher Res TROPOS, Leipzig, Germany.
[Mueller, D.] NASA, Langley Res Ctr, Sci Syst & Applicat Inc, Hampton, VA 23665 USA.
[Mueller, D.] Univ Hertfordshire, Dept Phys Astron & Math, Hatfield AL10 9AB, Herts, England.
[Omar, A. H.] NASA, Langley Res Ctr, Hampton, VA 23665 USA.
RP Tesche, M (reprint author), Stockholm Univ, Dept Appl Environm Sci ITM, Svante Arrhenius Vag 8, SE-11418 Stockholm, Sweden.
EM matthias.tesche@itm.su.se
RI Wandinger, Ulla/E-3348-2014; MUELLER, DETLEF/F-1010-2015; Omar,
Ali/D-7102-2017;
OI MUELLER, DETLEF/0000-0002-0203-7654; Omar, Ali/0000-0003-1871-9235;
Tesche, Matthias/0000-0003-0096-4785
FU Deutsche Forschungsgemeinschaft (DFG) [FOR 539]
FX We like to thank Mark Vaughan for his help and criticism regarding the
present paper. The SAMUM research group was funded by the Deutsche
Forschungsgemeinschaft (DFG) under grant FOR 539. CALIPSO data used in
this study were obtained from the NASA Langley Research Center
Atmospheric Science Data Center (http://eosweb.larc.nasa.gov).
NR 48
TC 26
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U1 3
U2 17
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-897X
J9 J GEOPHYS RES-ATMOS
JI J. Geophys. Res.-Atmos.
PD APR 16
PY 2013
VL 118
IS 7
BP 2889
EP 2902
DI 10.1002/jgrd.50248
PG 14
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 153QT
UT WOS:000319618300016
ER
PT J
AU Nicolae, D
Nemuc, A
Muller, D
Talianu, C
Vasilescu, J
Belegante, L
Kolgotin, A
AF Nicolae, D.
Nemuc, A.
Mueller, D.
Talianu, C.
Vasilescu, J.
Belegante, L.
Kolgotin, A.
TI Characterization of fresh and aged biomass burning events using
multiwavelength Raman lidar and mass spectrometry
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
DE biomass burning aerosols; lidar; AMS; aerosol microphysical properties;
aerosol mass spectrometry
ID MICROPHYSICAL PARTICLE PARAMETERS; AEROSOL OPTICAL-PROPERTIES;
BACKSCATTER LIDAR; SMOKE; REGULARIZATION; EXTINCTION; INVERSION;
RETRIEVAL; AIRCRAFT; CAMPAIGN
AB This paper focuses on optical and microphysical properties of long-range transported biomass burning (BB) aerosols and their variation with atmospheric evolution (ageing), as observed by a multiwavelength Raman lidar, part of EARLINET (European Aerosol LIdar NETwork). Chemical analysis of the atmospheric aerosol was done using a colocated aerosol mass spectrometer (AMS). One relevant optical parameter for the ageing process is the angstrom ngstrom exponent. In our study, we find that it decreases from 2 for fresh to 1.4-0.5 for aged smoke particles. The ratio of lidar (extinction-to-backscatter) ratios (LR532/LR355) changes rapidly from values <1 for fresh to >1 for aged particles. The imaginary part of the refractive index is the most sensitive microphysical parameter. It decreases sharply from 0.05 to less than 0.01 for fresh and aged smoke particles, respectively. Single-scattering albedo (SSA) varies from 0.74 to 0.98 depending on aerosol age and source. The AMS was used to measure the marker ions of wood-burning particles during 2 days of measurements when the meteorological conditions favored the downward mixing of aerosols from lofted layers. Particle size distribution and particle effective radius from both AMS and lidar are similar, i.e., particle effective radii were approximately 0.27 mu m for fresh BB aerosol particles. Microphysical aerosol properties from inversion of the lidar data agree with similar studies carried out in different regions on the globe. Our study shows that the angstrom ngstrom exponent LR532/LR355 and the imaginary part of the refractive index can be used to clearly distinguish between fresh and aged smoke particles.
C1 [Nicolae, D.; Nemuc, A.; Talianu, C.; Vasilescu, J.; Belegante, L.] Natl Inst Res & Dev Optoelect, RO-77125 Magurele, Ilfov, Romania.
[Mueller, D.] Leibniz Inst Tropospher Res IfT, Leipzig, Germany.
[Mueller, D.] GIST, Kwangju, South Korea.
[Mueller, D.] NASA, Langley Res Ctr, Hampton, VA 23665 USA.
[Kolgotin, A.] Phys Instrumentat Ctr, Moscow, Russia.
RP Nemuc, A (reprint author), Natl Inst Res & Dev Optoelect, 409 Atomistilor St, RO-77125 Magurele, Ilfov, Romania.
EM anca@inoe.ro
RI Vasilescu, Jeni/C-2336-2011; Belegante, Livio/B-5812-2012; MUELLER,
DETLEF/F-1010-2015; Nicolae, Doina/I-4999-2016
OI MUELLER, DETLEF/0000-0002-0203-7654;
FU Romanian National Authority for Scientific Research, CNCS-UEFISCDI
[PN-II-RU-PD-2011-3-0082, PN 09-27 01 03]; European Community
[262254-ACTRIS]; Korea Meteorological Administration Research and
Development Program [CATER 2012-7080]
FX This work was supported by a grant of the Romanian National Authority
for Scientific Research, CNCS-UEFISCDI, project no.
PN-II-RU-PD-2011-3-0082 and grant no. PN 09-27 01 03 and by the European
Community's FP7-INFRASTRUCTURES-2010-1 under grant agreement no.
262254-ACTRIS. This work was also funded by the Korea Meteorological
Administration Research and Development Program under grant CATER
2012-7080.
NR 57
TC 19
Z9 19
U1 5
U2 34
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-897X
EI 2169-8996
J9 J GEOPHYS RES-ATMOS
JI J. Geophys. Res.-Atmos.
PD APR 16
PY 2013
VL 118
IS 7
BP 2956
EP 2965
DI 10.1002/jgrd.50324
PG 10
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 153QT
UT WOS:000319618300020
ER
PT J
AU Eriksson, S
Rastatter, L
AF Eriksson, S.
Rastaetter, L.
TI Alfven Mach number and IMF clock angle dependencies of sunward flow
channels in the magnetosphere
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
ID FLUX-TRANSFER EVENTS; FIELD; SASH
AB Interplanetary coronal mass ejections associated with strong interplanetary magnetic field (IMF) By have been shown to enhance the neutral density in low Earth orbit. The enhancement has been linked to strong downward Poynting fluxes embedded within ionospheric channels of significant sunward ExB drift (2000-3000 m/s). Here we present MHD results describing the magnetospheric counterpart of the ionospheric flow channel that Defense Meteorological Satellite Program (DMSP) encountered on 15 May 2005. It is shown that the clock angle of maximum sunward flow (theta(FC)) depends on the IMF clock angle theta(FC) = alpha * theta(IMF) -1.3 degrees with alpha = (0.30, 0.38, 0.43, 0.45) at X = (4, 2, 0, -2) R-E. This is poleward of the magnetic null point region. The flow also depends on the solar wind Alfven Mach number Vx = Vx0 - delta v * M-A. The critical M-A = Vx0 / delta V for Vx = 0 decreases from M-A = 3.42 (X = 4 R-E) to M-A = 2.40 (X = -2 R-E). The low M-A and theta(IMF) conditions that characterized the X = 2 RE flow and resulted in strong Poynting flux occurred for 16% of all 167 h in 1998-2008 with Dst < -180 nT.
C1 [Eriksson, S.] Univ Colorado, Lab Atmospher & Space Phys, Boulder, CO 80309 USA.
[Rastaetter, L.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Eriksson, S (reprint author), Univ Colorado, Lab Atmospher & Space Phys, Boulder, CO 80309 USA.
EM eriksson@lasp.colorado.edu
RI Rastaetter, Lutz/D-4715-2012;
OI Rastaetter, Lutz/0000-0002-7343-4147; Eriksson,
Stefan/0000-0002-5619-1577
FU NSF [AGS-1144154]
FX S.E. acknowledges support by NSF grant AGS-1144154.
NR 21
TC 4
Z9 4
U1 0
U2 5
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0094-8276
J9 GEOPHYS RES LETT
JI Geophys. Res. Lett.
PD APR 16
PY 2013
VL 40
IS 7
DI 10.1002/grl.50307
PG 6
WC Geosciences, Multidisciplinary
SC Geology
GA 148BP
UT WOS:000319217600001
ER
PT J
AU Knipp, D
Kilcommons, L
Hunt, L
Mlynczak, M
Pilipenko, V
Bowman, B
Deng, Y
Drake, K
AF Knipp, D.
Kilcommons, L.
Hunt, L.
Mlynczak, M.
Pilipenko, V.
Bowman, B.
Deng, Y.
Drake, K.
TI Thermospheric damping response to sheath-enhanced geospace storms
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
ID ION-CYCLOTRON WAVES; NITRIC-OXIDE; SABER EXPERIMENT; PLASMA SHEET;
SOLAR-WIND; ART.; DENSITY; CHAMP; MODEL
AB We show evidence that solar wind density enhancements and pressure pulses can lead to intense low-energy particle precipitation and an associated, but unexpected, damping of thermospheric density response. Ground-based indices, used as proxies for thermospheric energy deposition, fail to capture these interactions in forecasting algorithms. Superposed epoch comparison of a group of poorly specified neutral density storms suggests an event-chain of (1) multi-hour, pre-storm solar wind density enhancement, followed by solar wind dynamic pressure pulses that trigger excess low-energy particle flux to the upper atmosphere; (2) enhanced production of thermospheric Nitric Oxide (NO) by precipitating particles and storm heating; (3) NO infrared cooling and damping of the thermosphere; and (4) mis-forecast of neutral density. In the control storms, these features are absent or muted. We discuss the roles of solar wind pre-conditioning and solar cycle dependency in the problem storms. These problem neutral-density storms reveal an element of "geo-effectiveness" that highlights competition between hydrodynamic aspects of the solar wind and other interplanetary drivers.
C1 [Knipp, D.; Kilcommons, L.] Univ Colorado, Boulder, CO 80309 USA.
[Knipp, D.] NCAR, High Altitude Observ, Boulder, CO USA.
[Knipp, D.] Space Environm Technol, Pacific Palisades, CA USA.
[Hunt, L.] Sci Syst & Applicat Inc, Hampton, VA USA.
[Mlynczak, M.] NASA, Sci Directorate, Langley Res Ctr, Hampton, VA USA.
[Pilipenko, V.] Space Res Inst, Moscow, Russia.
[Bowman, B.] USAF, Space Command, Colorado Springs, CO USA.
[Deng, Y.] Univ Texas Arlington, Dept Phys, Arlington, TX USA.
RP Knipp, D (reprint author), Univ Colorado, Boulder, CO 80309 USA.
EM delores.knipp@colorado.edu
FU AFOSR [FA9550-07-1-0565]; NRC fellowship at NOAA's Space Weather
Prediction Center; [AFRL FA9453-12-1-0244]; [AFSOR FA9550-12-1-0264];
[NSFATM1025089]; [NSFATM0955629]; [AFOSR 1210429]; [MJE-NSF
ATM-0827903]
FX We are grateful to F. Rich, M. Engebretson, C. Lin, E. Sutton, G.
Wilson, E. Zesta, H. Luhr, W. Wang, S. Solomon, J. Raeder. R. Redmon, M.
G. McHarg, and A. Richmond for fruitful discussions. We used particle
data from the DMSP archive at the National Geophysical Data Center. We
made extensive use of the NASA OMNIweb database. Kyoto University,
Kyoto, Japan, provided Dst data to OMNIweb. The following grants
supported this work: DK and LK-AFRL FA9453-12-1-0244, AFSOR
FA9550-12-1-0264, and NSFATM1025089; YD-NSFATM0955629 and AFOSR 1210429;
and VP and MJE-NSF ATM-0827903. Early aspects of this work were
supported by AFOSR FA9550-07-1-0565 and an NRC fellowship at NOAA's
Space Weather Prediction Center to DK.
NR 38
TC 12
Z9 12
U1 0
U2 13
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0094-8276
J9 GEOPHYS RES LETT
JI Geophys. Res. Lett.
PD APR 16
PY 2013
VL 40
IS 7
DI 10.1002/grl.50197
PG 5
WC Geosciences, Multidisciplinary
SC Geology
GA 148BP
UT WOS:000319217600002
ER
PT J
AU Parkinson, CL
Comiso, JC
AF Parkinson, Claire L.
Comiso, Josefino C.
TI On the 2012 record low Arctic sea ice cover: Combined impact of
preconditioning and an August storm
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
ID DECLINE
AB A new record low Arctic sea ice extent for the satellite era, 3.4 x 10(6) km(2), was reached on 13 September 2012; and a new record low sea ice area, 3.0 x 10(6) km(2), was reached on the same date. Preconditioning through decades of overall ice reductions made the ice pack more vulnerable to a strong storm that entered the central Arctic in early August 2012. The storm caused the separation of an expanse of 0.4 x 10(6) km(2) of ice that melted in total, while its removal left the main pack more exposed to wind and waves, facilitating the main pack's further decay. Future summer storms could lead to a further acceleration of the decline in the Arctic sea ice cover and should be carefully monitored.
C1 [Parkinson, Claire L.; Comiso, Josefino C.] NASA, Cryospher Sci Lab, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Parkinson, CL (reprint author), NASA, Cryospher Sci Lab, Goddard Space Flight Ctr, Code 615, Greenbelt, MD 20771 USA.
EM Claire.L.Parkinson@nasa.gov
RI Parkinson, Claire/E-1747-2012
OI Parkinson, Claire/0000-0001-6730-4197
FU Cryospheric Sciences Program at NASA Headquarters
FX The authors thank Rob Gersten of ADNET/RSIS and Larry Stock of SGT for
their support in the creation of the figures and the Cryospheric
Sciences Program at NASA Headquarters for funding the work. They also
thank Ian Simmonds and Harry Stern for many valuable comments on the
manuscript.
NR 36
TC 124
Z9 130
U1 4
U2 60
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0094-8276
EI 1944-8007
J9 GEOPHYS RES LETT
JI Geophys. Res. Lett.
PD APR 16
PY 2013
VL 40
IS 7
DI 10.1002/grl.50349
PG 6
WC Geosciences, Multidisciplinary
SC Geology
GA 148BP
UT WOS:000319217600019
ER
PT J
AU Richter, N
Poland, MP
Lundgren, PR
AF Richter, Nicole
Poland, Michael P.
Lundgren, Paul R.
TI TerraSAR-X interferometry reveals small-scale deformation associated
with the summit eruption of Kilauea Volcano, Hawai'i
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
AB On 19 March 2008, a small explosive eruption at the summit of Kilauea Volcano, Hawai'i, heralded the formation of a new vent along the east wall of Halema'uma'u Crater. In the ensuing years, the vent widened due to collapses of the unstable rim and conduit wall; some collapses impacted an actively circulating lava pond and resulted in small explosive events. We used synthetic aperture radar data collected by the TerraSAR-X satellite, a joint venture between the German Aerospace Center (DLR) and EADS Astrium, to identify and analyze small-scale surface deformation around the new vent during 2008-2012. Lidar data were used to construct a digital elevation model to correct for topographic phase, allowing us to generate differential interferograms with a spatial resolution of about 3m in Kilauea's summit area. These interferograms reveal subsidence within about 100m of the rim of the vent. Small baseline subset time series analysis suggests that the subsidence rate is not constant and, over time, may provide an indication of vent stability and potential for rim and wall collapse-information with obvious hazard implications. The deformation is not currently detectable by other space- or ground-based techniques.
C1 [Richter, Nicole] Univ Jena, Dept Earth Observat, Jena, Germany.
[Lundgren, Paul R.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
RP Richter, N (reprint author), Univ Jena, Dept Earth Observat, Jena, Germany.
EM nrichter@gfz-potsdam.de
OI Poland, Michael/0000-0001-5240-6123
FU German Academic Exchange Service (DAAD); German Aerospace Center (DLR)
through the Hawaii Supersite [GEO0747, GEO0875]; National Aeronautics
and Space Administration at the Jet Propulsion Laboratory, California
Institute of Technology
FX We are grateful to Tim Orr for providing the vent area data. We also
thank Don Swanson, Rowena Lohman, and an anonymous referee for reviews
that improved the manuscript. This research was completed as part of
Richter's M. S. thesis at the University of Jena, supported by
Christiane Schmullius and with funding provided by the German Academic
Exchange Service (DAAD). The LIDAR data were provided by Adam Soule
(Woods Hole Oceanographic Institute). TerraSAR-X data were provided by
the German Aerospace Center (DLR) through the Hawaii Supersite (projects
GEO0747 and GEO0875). Part of the research described in this paper was
supported under contract with the National Aeronautics and Space
Administration at the Jet Propulsion Laboratory, California Institute of
Technology.
NR 15
TC 8
Z9 9
U1 1
U2 10
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0094-8276
J9 GEOPHYS RES LETT
JI Geophys. Res. Lett.
PD APR 16
PY 2013
VL 40
IS 7
DI 10.1002/grl.50286
PG 5
WC Geosciences, Multidisciplinary
SC Geology
GA 148BP
UT WOS:000319217600005
ER
PT J
AU Periyakaruppan, A
Gandhiraman, RP
Meyyappan, M
Koehne, JE
AF Periyakaruppan, Adaikkappan
Gandhiraman, Ram P.
Meyyappan, M.
Koehne, Jessica E.
TI Label-Free Detection of Cardiac Troponin-I Using Carbon Nanofiber Based
Nanoelectrode Arrays
SO ANALYTICAL CHEMISTRY
LA English
DT Article
ID ELECTROCHEMICAL IMPEDANCE SPECTROSCOPY; PROTEIN ADSORPTION; BIOSENSORS;
MYOGLOBIN; BIOCHIPS; ANTIBODY; SERUM
AB A label-free biosensor is presented using carbon nanofiber (CNF) nanoelectrode arrays for the detection of cardiac troponin-I in the early diagnosis of myocardial infarction. Immobilization of anti-cTnI Ab on CNFs and the detection of human-cTnI were examined using electrochemical impedance spectroscopy and cyclic voltammetry techniques. Each step of the modification process was monitored, and the results show changes in electrical capacitance or resistance to charge transfer due to the specificity of corresponding adsorption of Ab-Ag interaction. The immunosensor demonstrates a good selectivity and high sensitivity against human-cTnI analytes and is capable of detecting cTnI at concentrations as low as similar to 0.2 ng/mL, which is 25 times lower than that possible by conventional methods. Analysis of the electrode at various stages using atomic force microscopy and X-ray reflectivity provides information on the surface roughness and orientation of the antibody.
C1 [Periyakaruppan, Adaikkappan; Gandhiraman, Ram P.; Meyyappan, M.; Koehne, Jessica E.] NASA, Ctr Nanotechnol, Ames Res Ctr, Moffett Field, CA 94035 USA.
RP Koehne, JE (reprint author), NASA, Ctr Nanotechnol, Ames Res Ctr, Moffett Field, CA 94035 USA.
EM jessica.e.koehne@nasa.gov
RI Gandhiraman, Ram Prasad/B-7004-2013
OI Gandhiraman, Ram Prasad/0000-0001-8957-7938
FU NASA URC [NNX08BA47A]; Science Foundation Ireland [10/CE/B1821-STTF 11]
FX A.P. acknowledges Dr. Olufisayo Jejelowo and Dr. Adebayo Oyekan of Texas
Southern University and Dr. Govindarajan Ramesh of Norfolk State
University for their support. A.P. is a visiting Postdoctoral Fellow
from TSU, Houston, supported by a NASA URC contract to TSU (NNX08BA47A).
R.P.G. is a visiting research scholar from Dublin City University,
Ireland under the Science Foundation Ireland fellowship 10/CE/B1821-STTF
11. The authors acknowledge Dr. Apurva Mehta and Dr. Michael F. Toney
from Stanford Synchrotron Radiation Light Source (SSRL), Stanford
University for their help in X ray reflectivity measurement.
NR 35
TC 46
Z9 46
U1 7
U2 95
PU AMER CHEMICAL SOC
PI WASHINGTON
PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA
SN 0003-2700
EI 1520-6882
J9 ANAL CHEM
JI Anal. Chem.
PD APR 16
PY 2013
VL 85
IS 8
BP 3858
EP 3863
DI 10.1021/ac302801z
PG 6
WC Chemistry, Analytical
SC Chemistry
GA 128UI
UT WOS:000317794800012
PM 23384128
ER
PT J
AU Rand, E
Periyakaruppan, A
Tanaka, Z
Zhang, DA
Marsh, MP
Andrews, RJ
Lee, KH
Chen, B
Meyyappan, M
Koehne, JE
AF Rand, Emily
Periyakaruppan, Adaikkappan
Tanaka, Zuki
Zhang, David A.
Marsh, Michael P.
Andrews, Russell J.
Lee, Kendall H.
Chen, Bin
Meyyappan, M.
Koehne, Jessica E.
TI A carbon nanofiber based biosensor for simultaneous detection of
dopamine and serotonin in the presence of ascorbic acid
SO BIOSENSORS & BIOELECTRONICS
LA English
DT Article
DE Biosensor; Dopamine; Serotonin; Carbon nanofiber; Nanoelectrode array
ID NANOTUBE NANOELECTRODE ARRAYS; ELECTROCHEMICAL DETECTION; URIC-ACID;
ELECTRODES; FILM; BRAIN; MICROELECTRODES; VOLTAMMETRY; SELECTIVITY;
FABRICATION
AB A biosensor based on an array of vertically aligned carbon nanofibers (CNFs) grown by plasma enhanced chemical vapor deposition is found to be effective for the simultaneous detection of dopamine (DA) and serotonin (5-HT) in the presence of excess ascorbic acid (AA). The CNF electrode outperforms the conventional glassy carbon electrode (GCE) for both selectivity and sensitivity. Using differential pulse voltammetry (DPV), three distinct peaks are seen for the CNF electrode at 0.13 V, 0.45 V, and 0.70 V for the ternary mixture of AA, DA, and 5-HT. In contrast, the analytes are indistinguishable in a mixture using a GCE. For the CNF electrode, the detection limits are 50 nM for DA and 250 nM for 5-HT. Published by Elsevier B.V.
C1 [Rand, Emily; Periyakaruppan, Adaikkappan; Zhang, David A.; Andrews, Russell J.; Chen, Bin; Meyyappan, M.; Koehne, Jessica E.] NASA, Ames Res Ctr, Ctr Nanotechnol, Moffett Field, CA 94035 USA.
[Tanaka, Zuki; Chen, Bin] Univ Calif Santa Cruz, Dept Elect Engn, Santa Cruz, CA 95064 USA.
[Marsh, Michael P.; Lee, Kendall H.] Mayo Clin, Dept Neurosurg, Rochester, MN 55905 USA.
[Lee, Kendall H.] Mayo Clin, Dept Physiol & Biomed Engn, Rochester, MN 55905 USA.
RP Koehne, JE (reprint author), NASA, Ames Res Ctr, Ctr Nanotechnol, Moffett Field, CA 94035 USA.
EM Jessica.E.Koehne@nasa.gov
RI Periyakaruppan, Adaikkappan/B-7398-2013
OI Periyakaruppan, Adaikkappan/0000-0002-0395-6564
FU NIH [R01-NS75013]; NASA URC Contract [NNx08BA47A]
FX This work was in part supported by an NIH Grant (R01-NS75013) to Mayo
Clinic. AP was supported by a NASA URC Contract to Texas Southern
University (NNx08BA47A) as a visiting Postdoctoral Fellow. The authors
would like to thank Patrick Wilhite and Anshul Vyas of Santa Clara
University for helpful discussions regarding carbon nanofiber growth.
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PU ELSEVIER ADVANCED TECHNOLOGY
PI OXFORD
PA OXFORD FULFILLMENT CENTRE THE BOULEVARD, LANGFORD LANE, KIDLINGTON,
OXFORD OX5 1GB, OXON, ENGLAND
SN 0956-5663
J9 BIOSENS BIOELECTRON
JI Biosens. Bioelectron.
PD APR 15
PY 2013
VL 42
BP 434
EP 438
DI 10.1016/j.bios.2012.10.080
PG 5
WC Biophysics; Biotechnology & Applied Microbiology; Chemistry, Analytical;
Electrochemistry; Nanoscience & Nanotechnology
SC Biophysics; Biotechnology & Applied Microbiology; Chemistry;
Electrochemistry; Science & Technology - Other Topics
GA 158EH
UT WOS:000319951700072
PM 23228495
ER
PT J
AU Yamaguchi, A
Mikouchi, T
Ito, M
Shirai, N
Barrat, JA
Messenger, S
Ebihara, M
AF Yamaguchi, A.
Mikouchi, T.
Ito, M.
Shirai, N.
Barrat, J. A.
Messenger, S.
Ebihara, M.
TI Experimental evidence of fast transport of trace elements in planetary
basaltic crusts by high temperature metamorphism
SO EARTH AND PLANETARY SCIENCE LETTERS
LA English
DT Article
DE elemental transport; planetary basalts; metamorphism; geochemistry;
chronology
ID RARE-EARTH ELEMENTS; METEORITE SAMPLES; ION MICROPROBE; EUCRITES;
DIFFUSION; ABUNDANCES; EVOLUTION; MIGRATION; HISTORY; IMPACT
AB Incompatible elements (IEs) such as K, P, Ti, and rare earth elements (REEs) provide important constraints on the geochemistry and chronology of basaltic meteorites, most of which experienced complicated post-crystallization histories. These elements are immobile under subsolidus conditions because of their slow diffusion rates in planetary basalt minerals such as pyroxene and plagioclase. Thus, IEs are considered to preserve in most cases, reliable records of formation processes, even in ancient rocks that have undergone moderate thermal processing. However, observations of natural planetary samples suggest that melting of IE accessory carrier phases enhances the mobilization of such elements. Here we show that IEs are rapidly transported by near-solidus partial melting of highly IE-enriched minor phases including Ca-phosphate and Ti-rich phases. These partial melts occur as interconnected veins along cracks and fractures, and as thin films on surfaces of pore spaces, indicating that the melt mobilization is driven by surface tension. The melt transport provides the necessary condition for melt migration consistent with the presence of the depleted basaltic eucrites. Also, reaction between major minerals pyroxene and plagioclase, and partial melts may cause disturbance and resetting of some isotopic systems. These results have important implications for a range of geochemical investigations. In particular, the elemental fractionation resulting from such partial melting may result in improper age determinations. (C) 2013 Elsevier B.V. All rights reserved.
C1 [Yamaguchi, A.] Natl Inst Polar Res, Tachikawa, Tokyo 1908518, Japan.
[Yamaguchi, A.] Grad Univ Adv Sci, Sch Multidisciplinary Sci, Dept Polar Sci, Tachikawa, Tokyo 1908518, Japan.
[Mikouchi, T.] Univ Tokyo, Dept Earth & Planetary Sci, Tokyo 1130033, Japan.
[Ito, M.] USRA Houston, Lunar & Planetary Inst, Houston, TX 77058 USA.
[Ito, M.; Messenger, S.] NASA, Robert M Walker Lab Space Sci, Lyndon B Johnson Space Ctr, ARES, Houston, TX 77058 USA.
[Shirai, N.; Ebihara, M.] Tokyo Metropolitan Univ, Grad Sch Sci, Hachioji, Tokyo 1920397, Japan.
[Barrat, J. A.] Univ Europeenne Bretagne, UBO IUEM, CNRS UMR 6538, F-29280 Plouzane, France.
RP Yamaguchi, A (reprint author), Natl Inst Polar Res, Tachikawa, Tokyo 1908518, Japan.
EM yamaguch@nipr.ac.jp
FU Ministry of Education, Science, and Technology, Japan, NIPR [KP-6]; NASA
FX This work is partly supported by a Grant-in-Aid for Scientific Research
from Ministry of Education, Science, and Technology, Japan, NIPR
Research Project Funds, KP-6, and by a NASA Origins Program Grant to
S.M., and Cosmochemistry Program to S.M. and M.I. We thank reviewers, C.
Floss and anonymous reviewers for constructing reviews, and B. Marty for
editorial assistance.
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PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0012-821X
J9 EARTH PLANET SC LETT
JI Earth Planet. Sci. Lett.
PD APR 15
PY 2013
VL 368
BP 101
EP 109
DI 10.1016/j.epsl.2013.02.036
PG 9
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 160AH
UT WOS:000320087900011
ER
PT J
AU de Groot, WJ
Cantin, AS
Flannigan, MD
Soja, AJ
Gowman, LM
Newbery, A
AF de Groot, William J.
Cantin, Alan S.
Flannigan, Michael D.
Soja, Amber J.
Gowman, Lynn M.
Newbery, Alison
TI A comparison of Canadian and Russian boreal forest fire regimes
SO FOREST ECOLOGY AND MANAGEMENT
LA English
DT Article
DE Carbon emissions; Fire behaviour; Fire ecology; Fire weather; Fuels
ID CROWN FIRE; MANAGEMENT; SYSTEM
AB Boreal forest dynamics are largely driven by disturbance, and fire is a prevalent force of change across the boreal circumpolar region. North American and Eurasian boreal fire regimes are known to be very different but there are few quantitative comparison studies. Russian and Canadian boreal fire regimes are compared using fire weather, fire statistics, fire behaviour, and C emissions data from two large study areas. Fuel consumption, head fire intensity, and C emissions were modelled using fire weather data, fuels data and burned area polygons for all large (200+ ha) fires that occurred in the study areas during 2001-2007. Fire behaviour and C emissions of each large fire were simulated with the Canadian Fire Effects Model (CanFIRE) using fuel type and fuel load data of the burned areas, and Canadian Forest Fire Weather Index System parameters, as interpolated to the fire from the weather station network on the average active fire date. In the Russian study area located in central Siberia, there was an annual average of 1441.9 large fires per 100 M ha of forest land that burned 1.89 M ha (average large fire size = 1312 ha, mean fire return interval = 52.9 years) with an average fire intensity of 4858 kW m(-1). In the western Canada study area, there was an annual average of 93.7 large fires per 100 M ha of forest land that burned 0.56 M ha of forest (average large fire size = 5930 ha, mean fire return interval = 179.9 years) with an average fire intensity of 6047 kW m(-1). The 2001-2007 fire size distribution and annual area burned in the Canadian study area were very similar to 1970-2009 statistics, although large fire frequency was higher and average large fire size was smaller. Similar long-term fire statistics for Russia currently do not exist for comparison. The C emissions rate (t ha(-1) of burned area) was 53% higher in the Canadian study area due to higher pre-burn forest floor fuel loads and higher fuel consumption by crown fires. However, the Russian study area had much higher total C emissions (per 100 M ha of forest area) because of greater annual area burned. The Russian C emissions estimate in this study is likely conservative due to low forest floor fuel load estimates in available datasets. Fire regime differences are discussed in terms of fuel, weather, and fire ecology. Crown Copyright (C) 2012 Published by Elsevier B.V. All rights reserved.
C1 [de Groot, William J.; Cantin, Alan S.; Gowman, Lynn M.; Newbery, Alison] Canadian Forest Serv, Nat Resources Canada, Sault Ste Marie, ON P6A 2E5, Canada.
[Flannigan, Michael D.] Univ Alberta, Dept Renewable Resources, Edmonton, AB T6G 2H1, Canada.
[Soja, Amber J.] NASA, Natl Inst Aerosp, Langley Res Ctr, Climate Sci Branch, Hampton, VA 23681 USA.
[Soja, Amber J.] NASA, Natl Inst Aerosp, Langley Res Ctr, Chem & Dynam Branch, Hampton, VA 23681 USA.
RP de Groot, WJ (reprint author), Canadian Forest Serv, Nat Resources Canada, 1219 Queen St East, Sault Ste Marie, ON P6A 2E5, Canada.
EM bill.degroot@nrcan.gc.ca
RI Flannigan, Michael/G-6996-2015
OI Flannigan, Michael/0000-0002-9970-5363
FU USDA Forest Service; NASA Land Cover Land Use Change (LCLUC) program;
NASA Terrestrial Ecosystems (TE) program; NASA InterDisciplinary Science
(IDS) program
FX Ji-Zhong Jin provided historical fire weather data for Russia. Sara
Bennett conducted GIS analyses. Doug McRae, Brian Stocks, and Sue Canard
provided valuable expertise and advice. We gratefully acknowledge
support provided by the USDA Forest Service and NASA Land Cover Land Use
Change (LCLUC), Terrestrial Ecosystems (TE) and InterDisciplinary
Science (IDS) programs.
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PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0378-1127
J9 FOREST ECOL MANAG
JI For. Ecol. Manage.
PD APR 15
PY 2013
VL 294
SI SI
BP 23
EP 34
DI 10.1016/j.foreco.2012.07.033
PG 12
WC Forestry
SC Forestry
GA 125MW
UT WOS:000317544900004
ER
PT J
AU Fu, LL
Haines, BJ
AF Fu, Lee-Lueng
Haines, Bruce J.
TI The challenges in long-term altimetry calibration for addressing the
problem of global sea level change
SO ADVANCES IN SPACE RESEARCH
LA English
DT Article
DE Altimetry; Calibration; Sea level change
ID TOPEX MICROWAVE RADIOMETER; PRECISION ORBIT DETERMINATION; TERRESTRIAL
REFERENCE FRAME; CLIMATE DATA RECORD; SATELLITE ALTIMETRY; ABSOLUTE
CALIBRATION; TOPOGRAPHY MISSION; GEOCENTER MOTION; TOPEX/POSEIDON;
JASON-1
AB Long-term change of the global sea level resulting from climate change has become an issue of great societal interest. The advent of the technology of satellite altimetry has modernized the study of sea level on both global and regional scales. In combination with in situ observations of the ocean density and space observations of Earth's gravity variations, satellite altimetry has become an essential component of a global observing system for monitoring and understanding sea level change. The challenge of making sea level measurements with sufficient accuracy to discern long-term trends and allow the patterns of natural variability to be distinguished from those linked to anthropogenic forcing rests largely on the long-term efforts of altimeter calibration and validation. The issues of long-term calibration for the various components of the altimeter measurement system are reviewed in the paper. The topics include radar altimetry, the effects of tropospheric water vapor, orbit determination, gravity field, tide gauges, and the terrestrial reference frame. The necessity for maintaining a complete calibration effort and the challenges of sustaining it into the future are discussed. (C) 2012 COSPAR. Published by Elsevier Ltd. All rights reserved.
C1 [Fu, Lee-Lueng; Haines, Bruce J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Fu, LL (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM llf@jpl.nasa.gov; bruce.j.haines@jpl.nasa.gov
FU National Aeronautic and Space Administration; Jason-1 Project;
OSTM/Jason-2 Project
FX The research presented in the paper was carried out at the Jet
Propulsion Laboratory (JPL), California Institute of Technology, under
contract with the National Aeronautic and Space Administration. Support
from the Jason-1 and OSTM/Jason-2 Projects is acknowledged. We are
grateful for input from three anonymous reviewers, as well as Xiaoping
Wu, Shannon Brown and Shailen Desai at JPL.; (C) 2012 California
Institute of Technology. Government sponsorship acknowledged.
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PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND
SN 0273-1177
EI 1879-1948
J9 ADV SPACE RES
JI Adv. Space Res.
PD APR 15
PY 2013
VL 51
IS 8
BP 1284
EP 1300
DI 10.1016/j.asr.2012.06.005
PG 17
WC Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology &
Atmospheric Sciences
SC Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences
GA 129XZ
UT WOS:000317878600002
ER
PT J
AU Melachroinos, SA
Lemoine, FG
Zelensky, NP
Rowlands, DD
Luthcke, SB
Bordyugov, O
AF Melachroinos, S. A.
Lemoine, F. G.
Zelensky, N. P.
Rowlands, D. D.
Luthcke, S. B.
Bordyugov, O.
TI The effect of geocenter motion on Jason-2 orbits and the mean sea level
SO ADVANCES IN SPACE RESEARCH
LA English
DT Article
DE Jason-2; Geocenter motion; GPS; SLRIDORIS; Mean sea level error
ID TERRESTRIAL REFERENCE FRAME; GPS; MODEL; TOPEX/POSEIDON; TRACKING;
SERVICE; SERIES; DORIS; EARTH; SLR
AB We compute a series of Jason-2 GPS and SLR/DORIS-based orbits using ITRF2005 and the std0905 standards (Lemoine et al., 2010). Our GPS and SLR/DOR/S orbit data sets span a period of 2 years from cycle 3 (July 2008) to cycle 74 (July 2010). We extract the Jason-2 orbit frame translational parameters per cycle by the means of a Helmert transformation between a set of reference orbits and a set of test orbits. We compare the annual terms of these time-series to the annual terms of two different geocenter motion models where biases and trends have been removed. Subsequently, we include the annual terms of the modeled geocenter motion as a degree-1 loading displacement correction to the GPS and SLR/DORIS tracking network of the POD process. Although the annual geocenter motion correction would reflect a stationary signal in time, under ideal conditions, the whole geocenter motion is a non-stationary process that includes secular trends. Our results suggest that our GSFC Jason-2 GPS-based orbits are closely tied to the center of mass (CM) of the Earth consistent with our current force modeling, whereas GSFC's SLR/DORIS-based orbits are tied to the origin of ITRF2005, which is the center of figure (CF) for sub-secular scales. We quantify the GPS and SLR/DORIS orbit centering and how this impacts the orbit radial error over the globe, which is assimilated into mean sea level (MSL) error, from the omission of the annual term of the geocenter correction. We find that for the SLR/DORIS std0905 orbits, currently used by the oceanographic community, only the negligence of the annual term of the geocenter motion correction results in a - 4.67 +/- 3.40 mm error in the Z-component of the orbit frame which creates 1.06 +/- 2.66 mm of systematic error in the MSL estimates, mainly due to the uneven distribution of the oceans between the North and South hemisphere. (C) 2012 COSPAR. Published by Elsevier Ltd. All rights reserved.
C1 [Melachroinos, S. A.; Lemoine, F. G.; Zelensky, N. P.; Rowlands, D. D.; Luthcke, S. B.; Bordyugov, O.] NASA, Goddard Space Flight Ctr, Planetary Geodynam Branch, Greenbelt, MD 20771 USA.
[Melachroinos, S. A.; Zelensky, N. P.; Bordyugov, O.] SGT Inc, Greenbelt, MD USA.
RP Melachroinos, SA (reprint author), NASA, Goddard Space Flight Ctr, Planetary Geodynam Branch, Greenbelt, MD 20771 USA.
EM Smelachroinos@sgt-inc.com; Frank.G.Lemoine@nasa.gov
RI Lemoine, Frank/D-1215-2013; Rowlands, David/D-2751-2012
FU NASA [NNH09ZDA001N-IDS, NNH07ZDA001N-OSTST]
FX This research was supported by the following NASA Programs:
NNH09ZDA001N-IDS: Interdisciplinary Research in Earth Science (IDS) and
NNH07ZDA001N-OSTST: Ocean Surface Topography Science Team. We thank the
two anonymous reviewers, Dr. Xavier Collilieux and the editor Dr. Pascal
Willis for their constructive comments on this manuscript.
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PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND
SN 0273-1177
EI 1879-1948
J9 ADV SPACE RES
JI Adv. Space Res.
PD APR 15
PY 2013
VL 51
IS 8
BP 1323
EP 1334
DI 10.1016/j.asr.2012.06.004
PG 12
WC Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology &
Atmospheric Sciences
SC Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences
GA 129XZ
UT WOS:000317878600005
ER
PT J
AU Haines, BJ
Desai, SD
Born, GH
AF Haines, Bruce J.
Desai, Shailen D.
Born, George H.
TI GPS monitoring of vertical seafloor motion at Platform Harvest
SO ADVANCES IN SPACE RESEARCH
LA English
DT Article
DE GPS positioning; Altimeter calibration; Seafloor subsidence; Sea level
ID HEIGHT TIME-SERIES; ABSOLUTE CALIBRATION; CROSS-CALIBRATION; RADAR
ALTIMETERS; JASON-1; TOPEX/POSEIDON; SURFACE; SATELLITE; RECEIVER; PHASE
AB We describe results from two decades of monitoring vertical seafloor motion at the Harvest oil platform, NASA's prime verification site for the TOPEX/Poseidon and Jason series of reference altimeter missions. Using continuous GPS observations, we refine estimates of the platform subsidence due most likely to fluid withdrawal linked to oil production and describe the impact on estimates of stability for the altimeter measurement systems. The cumulative seafloor subsidence over 20 yrs is approximately 10 cm, but the rate does not appear constant. The apparent non-linear nature of the vertical motion, coupled with long-period GPS errors, implies that the quality of the seafloor motion estimates is not uniform over the 20-yr period. For the Jason-1 era (2002-2009), competing estimates for the subsidence show agreement to better than 1 mm yr(-1). Longer durations of data are needed before the seafloor motion estimates for the Jason-2 era (2008-present) can approach this level of accuracy. (C) 2012 COSPAR. Published by Elsevier Ltd. All rights reserved.
C1 [Haines, Bruce J.; Desai, Shailen D.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Born, George H.] Univ Colorado, Colorado Ctr Astrodynam Res, Boulder, CO 80310 USA.
RP Haines, BJ (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr,MIS 238-600, Pasadena, CA 91109 USA.
EM bruce.j.haines@jpl.nasa.gov
FU NASA
FX We are indebted to Dave Stowers (JPL) and UNAVCO for their support of
the GPS component of the Harvest experiment, and to Christina Selle
(JPL) for her significant efforts in reprocessing the historical GPS
data for improved orbit and clock products. The Harvest research
activities are funded by the NASA Physical Oceanography Program. We are
grateful to Eric Lindstrom and Lee Fu for advancing the Harvest
experiment and for assisting with the renewal of interagency agreements
needed for experiment upgrades. Production data for the Arguello
Reservoir were obtained from the U. S. Bureau of Ocean Energy
Management. We thank three anonymous reviewers for their comments and
suggestions, which have led to important improvements in the paper. A
portion of the work described in this paper was performed at the Jet
Propulsion Laboratory, California Institute of Technology under contract
with the National Aeronautics and Space Administration.
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PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND
SN 0273-1177
EI 1879-1948
J9 ADV SPACE RES
JI Adv. Space Res.
PD APR 15
PY 2013
VL 51
IS 8
BP 1369
EP 1382
DI 10.1016/j.asr.2012.11.008
PG 14
WC Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology &
Atmospheric Sciences
SC Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences
GA 129XZ
UT WOS:000317878600008
ER
PT J
AU Willis, P
Mertikas, S
Argus, DF
Bock, O
AF Willis, Pascal
Mertikas, Stelios
Argus, Don F.
Bock, Olivier
TI DORIS and GPS monitoring of the Gavdos calibration site in Crete
SO ADVANCES IN SPACE RESEARCH
LA English
DT Article
DE DORIS; GPS; Satellite altimetry calibration; Gavdos; Troposphere
ID ABSOLUTE CALIBRATION; PLATE KINEMATICS; CONSTRAINTS; SATELLITE; JASON-1;
TOPEX/POSEIDON; DEFORMATION; GRADIENTS; ITRF2008; NETWORK
AB Due to its specific geographical location as well as its geodetic equipment (DORIS, GNSS, microwave transponder and tide gauges), the Gavdos station in Crete, Greece is one of the very few sites around the world used for satellite altimetry calibration. To investigate the quality of the Gavdos geodetic coordinates and velocities, we analyzed and compared here DORIS and GPS-derived results obtained during several years of observations. The DORIS solution is the latest ignwd11 solution at IGN, expressed in ITRF2008, while the GPS solution was obtained using the GAMIT software package. Current results show that 1-2 mm/yr agreement can be obtained for 3-D velocity, showing a good agreement with current geophysical models. In particular, the agreement obtained for the vertical velocity is around 0.3-0.4 mm/yr, depending on the terrestrial reference frame. As a by-product of these geodetic GPS and DORIS results, Zenith Tropospheric Delays (ZTDs) estimations were also compared in 2010 between these two techniques, and compared to ECMWF values, showing a 6.6 mm agreement in dispersion without any significant difference between GPS and DORIS (with a 97.6% correlation), but with a 13-14 mm agreement in dispersion when comparing to ECMWF model (with only about 90% correlation for both techniques). These tropospheric delay estimations could also provide an external calibration of the tropospheric correction used for the geophysical data of satellite altimetry missions. (C) 2012 COSPAR. Published by Elsevier Ltd. All rights reserved.
C1 [Willis, Pascal] Inst Natl Informat Geog & Forestiere, Direct Tech, F-94165 St Mande, France.
[Willis, Pascal] UFR STEP, Inst Phys Globe Paris, PRES Sorbonne Paris Cite, F-75013 Paris, France.
[Mertikas, Stelios] Tech Univ Crete, Dept Mineral Resources Engn, Geodesy & Geomat Engn Lab, Khania 73100, Greece.
[Argus, Don F.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Bock, Olivier] Inst Natl Informat Geog & Forestiere, LAREG, F-77455 Marne La Vallee, France.
RP Willis, P (reprint author), Inst Natl Informat Geog & Forestiere, Direct Tech, 2 Ave Pasteur, F-94165 St Mande, France.
EM pascal.willis@ign.fr; mertikas@mred.tuc.gr; Donald.F.Argus@jpl.nasa.gov;
olivier.bock@ign.fr
RI Willis, Pascal/A-8046-2008
OI Willis, Pascal/0000-0002-3257-0679
FU National Aeronautics and Space Administration (NASA); FP7-REGPOT-2008-1
(SOFIA) [229885]; European Commission
FX This work was supported by the Centre National d'Etudes Spatiales
(CNES). It is based on observations with DORIS embarked on SPOTs,
TOPEX/Poseidon, Envisat, Jason-2 and Cryosat-2 satellites. Don Argus
performed research at Jet Propulsion Laboratory, under contract with the
National Aeronautics and Space Administration (NASA). This work has been
supported by the FP7-REG-POT-2008-1, Project No. 229885 (SOFIA),
sponsored by the European Commission. The help and support of Mr. X.
Frantzis for the GAMIT processing is much appreciated. This paper is
IPGP contribution number 3305.
NR 43
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PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND
SN 0273-1177
EI 1879-1948
J9 ADV SPACE RES
JI Adv. Space Res.
PD APR 15
PY 2013
VL 51
IS 8
BP 1438
EP 1447
DI 10.1016/j.asr.2012.08.006
PG 10
WC Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology &
Atmospheric Sciences
SC Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences
GA 129XZ
UT WOS:000317878600012
ER
PT J
AU Lowe, KT
Maisto, P
Byun, G
Simpson, RL
Verkamp, M
Danehy, PM
Tiemsin, PI
Wohl, CJ
AF Lowe, K. Todd
Maisto, Pietro
Byun, Gwibo
Simpson, Roger L.
Verkamp, Max
Danehy, Paul M.
Tiemsin, Pacita I.
Wohl, Christopher J.
TI Laser velocimetry with fluorescent dye-doped polystyrene microspheres
SO OPTICS LETTERS
LA English
DT Article
AB Simultaneous Mie scattering and laser-induced fluorescence (LIF) signals are obtained from individual polystyrene latex microspheres dispersed in an air flow. Microspheres less than 1 mu m mean diameter were doped with two organic fluorescent dyes, Rhodamine B (RhB) and dichlorofluorescein (DCF), intended either to provide improved particle-based flow velocimetry in the vicinity of surfaces or to provide scalar flow information (e. g., marking one of two fluid streams). Both dyes exhibit measureable fluorescence signals that are on the order of 10(-3) to 10(-4) times weaker than the simultaneously measured Mie signals. It is determined that at the conditions measured, 95.5% of RhB LIF signals and 32.2% of DCF signals provide valid laser-Doppler velocimetry measurements compared with the Mie scattering validation rate with 6.5 W of 532 nm excitation, while RhB excited with 1.0 W incident laser power still exhibits 95.4% valid velocimetry signals from the LIF channel. The results suggest that the method is applicable to wind tunnel measurements near walls where laser flare can be a limiting factor and monodisperse particles are essential.
C1 [Lowe, K. Todd; Maisto, Pietro] Virginia Tech Univ, Dept Aerosp & Ocean Engn, Blacksburg, VA 24061 USA.
[Byun, Gwibo; Simpson, Roger L.] AUR Inc, Blacksburg, VA 24060 USA.
[Verkamp, Max; Danehy, Paul M.; Tiemsin, Pacita I.; Wohl, Christopher J.] NASA, Langley Res Ctr, Hampton, VA 23681 USA.
RP Lowe, KT (reprint author), Virginia Tech Univ, Dept Aerosp & Ocean Engn, Blacksburg, VA 24061 USA.
EM kelowe@vt.edu
FU NASA ARMD Seedling Fund; NIA Cooperative Agreement [NNL09AA00A]
FX The authors acknowledge the support of the NASA ARMD Seedling Fund and
NIA Cooperative Agreement NNL09AA00A.
NR 10
TC 2
Z9 2
U1 3
U2 29
PU OPTICAL SOC AMER
PI WASHINGTON
PA 2010 MASSACHUSETTS AVE NW, WASHINGTON, DC 20036 USA
SN 0146-9592
J9 OPT LETT
JI Opt. Lett.
PD APR 15
PY 2013
VL 38
IS 8
BP 1197
EP 1199
PG 3
WC Optics
SC Optics
GA 125ZG
UT WOS:000317580200004
PM 23595429
ER
PT J
AU Odom, B
AF Odom, Brian
TI Encyclopedia of the US Presidency: A Historical Reference
SO LIBRARY JOURNAL
LA English
DT Book Review
C1 [Odom, Brian] NASA, Marshall Space & Flight Ctr, Huntsville, AL 35811 USA.
RP Odom, B (reprint author), NASA, Marshall Space & Flight Ctr, Huntsville, AL 35811 USA.
NR 1
TC 0
Z9 0
U1 0
U2 0
PU REED BUSINESS INFORMATION
PI NEW YORK
PA 360 PARK AVENUE SOUTH, NEW YORK, NY 10010 USA
SN 0363-0277
J9 LIBR J
JI Libr. J.
PD APR 15
PY 2013
VL 138
IS 7
BP 110
EP 110
PG 1
WC Information Science & Library Science
SC Information Science & Library Science
GA 124IW
UT WOS:000317458000253
ER
PT J
AU Yao, YJ
Liang, SL
Cheng, J
Liu, SM
Fisher, JB
Zhang, XD
Jia, K
Zhao, X
Qing, QM
Zhao, B
Han, SJ
Zhou, GS
Zhou, GY
Li, YL
Zhao, SH
AF Yao, Yunjun
Liang, Shunlin
Cheng, Jie
Liu, Shaomin
Fisher, Joshua B.
Zhang, Xudong
Jia, Kun
Zhao, Xiang
Qing, Qiming
Zhao, Bin
Han, Shijie
Zhou, Guangsheng
Zhou, Guoyi
Li, Yuelin
Zhao, Shaohua
TI MODIS-driven estimation of terrestrial latent heat flux in China based
on a modified Priestley-Taylor algorithm
SO AGRICULTURAL AND FOREST METEOROLOGY
LA English
DT Article
DE Latent heat flux; Evapotranspiration; Priestley-Taylor; MODIS; China
ID SURFACE-ENERGY BALANCE; NET PRIMARY PRODUCTION; AMAZON RAIN-FORESTS;
REMOTE-SENSING DATA; EVAPOTRANSPIRATION ALGORITHM; COMBINATION THEORY;
THERMAL INERTIA; CARBON-DIOXIDE; SATELLITE DATA; LAND SURFACES
AB Because of China's large size, satellite observations are necessary for estimation of the land surface latent heat flux (LE). We describe here a satellite-driven Priestley-Taylor (PT)-based algorithm constrained by the Normalized Difference Vegetation Index (NDVI) and Apparent Thermal Inertia (ATI) derived from temperature change over time. We compare to the satellite-driven PT-based approach, PT-JPL, and validate both models using data collected from 16 eddy covariance flux towers in China. Like PT-JPL, our proposed algorithm avoids the computational complexities of aerodynamic resistance parameters. We run the algorithms with monthly Moderate Resolution Imaging Spectroradiometer (MODIS) products (0.05 degrees resolution), including albedo, Land Surface Temperature (LST), surface emissivity, and NDVI; and, Insolation from the Japan Aerospace Exploration Agency (JAXA). We find good agreement between our estimates of monthly LE and field-measured LE, with respective Root Mean Square Error (RMSE) and bias differences of 12.5 Wm(-2) and -6.4Wm(-2). As compared with PT-JPL, our proposed algorithm has higher correlations with ground-measurements. Between 2001 and 2010, LE shows generally negative trends in most regions of China, though positive LE trends occur over 39% of the region, primarily in Northeast, North and South China. Our results indicate that the variations of terrestrial LE are responding to large-scale droughts and afforestation caused by human activity with direct links to terrestrial energy exchange, both spatially and temporally. (C) 2012 Elsevier B.V. All rights reserved.
C1 [Yao, Yunjun; Liang, Shunlin; Cheng, Jie; Jia, Kun; Zhao, Xiang] Beijing Normal Univ, State Key Lab Remote Sensing Sci, Beijing 100875, Peoples R China.
[Yao, Yunjun; Liang, Shunlin; Cheng, Jie; Jia, Kun; Zhao, Xiang] Chinese Acad Sci, Inst Remote Sensing Applicat, Beijing, Peoples R China.
[Yao, Yunjun; Liang, Shunlin; Cheng, Jie; Jia, Kun; Zhao, Xiang] Beijing Normal Univ, Coll Global Change & Earth Syst Sci, Beijing 100875, Peoples R China.
[Liang, Shunlin] Univ Maryland, Dept Geog Sci, College Pk, MD 20742 USA.
[Liu, Shaomin] Beijing Normal Univ, Sch Geog, State Key Lab Remote Sensing Sci, Beijing 100875, Peoples R China.
[Fisher, Joshua B.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Zhang, Xudong] Chinese Acad Forestry, Inst Forestry, Beijing 100091, Peoples R China.
[Qing, Qiming] Peking Univ, Inst Remote Sensing & GIS, Beijing 100871, Peoples R China.
[Zhao, Bin] Fudan Univ, Minist Educ Key Lab Biodivers Sci & Ecol Engn, Shanghai 200433, Peoples R China.
[Han, Shijie] Chinese Acad Sci, Inst Appl Ecol, Shenyang 110016, Peoples R China.
[Zhou, Guangsheng] Chinese Acad Sci, Inst Bot, Lab Quantitat Vegetat Ecol, Beijing 100093, Peoples R China.
[Zhou, Guoyi; Li, Yuelin] Chinese Acad Sci, South China Bot Garden, Guangzhou 510650, Guangdong, Peoples R China.
[Zhao, Shaohua] Environm Satellite Ctr, Minist Environm Protect, Beijing 100094, Peoples R China.
RP Yao, YJ (reprint author), Beijing Normal Univ, Coll Global Change & Earth Syst Sci, Beijing 100875, Peoples R China.
EM boyyunjun@163.com
RI Zhao, Bin/E-5349-2010; Zhao, Bin/I-3651-2013; Li, Yuelin/D-7249-2011;
Cheng, Jie/G-2039-2011; liang, shunlin/C-2809-2015; rslab,
water/O-7043-2015;
OI Zhao, Bin/0000-0002-3530-2469; Fisher, Joshua/0000-0003-4734-9085
FU Special Foundation for Free Exploration of State Laboratory of Remote
Sensing Science [ZY12-11]; Natural Science Fund of China [41201331,
40901167, 41101313]; High-Tech Research and Development Program of China
[2009AA122100]; Advance Research Program of Civil Aerospace Technology
FX The authors thank the anonymous reviewers for their critical and helpful
comments and suggestions. The authors would like to thank Dr. Xianhong
Xie, Dr. Wenping Yuan, Dr. Xianglan Li, Dr. Xiaotong Zhang, Dr. Bo Jiang
and Dr. Liang Sun from the College of Global Change and Earth System
Science, Beijing Normal University, China, for their suggestions. The
authors would like to thank Dr. Qibing Wang from the State Key Labratory
of Vegetation and Environmental Change, Institute of Botany, Chinese
Academy of Sciences, for his help. The authors would also like to extend
their thanks to China Meteorological Administration (CMA) for providing
ground-measured meteorological data. Latent heat flux, net radiation,
shortwave solar radiation and corresponding meteorological observations
were obtained from the Coordinated Enhanced Observation Project (CEOP)
in arid and semi-arid regions of northern China
(http://observation.tea.ac.cn/), the water experiments of Environmental
and Ecological Science Data Center for West China
(http://westdc.westgis.ac.cn/water), the Atmosphere Radiation
Measurement (ARM) Program of the U.S. Department of Energy
(http://www.archive.arm.gov/), the ChinaFlux network
(http://www.chinaflux.org/index/index.asp), the Japan Aerospace
Exploration Agency (JAXA)
(http://suzaku.eorcjaxajp/GLI/data/final/landpar/index.html). DEM data
was derived from Shuttle Radar Topography Mission (STRM) DEM data
(http://datamirror.csdb.cn/dem/searchjsp). The monthly PDSI products
were derived from the NCAR CGD's Climate Analysis Section dataset
(http://www.cgd.ucar.edu/cas/catalog/cljmind/pdsi.html). MODIS NDVI,
LST, albedo and land cover satellite products were obtained online
(http://reverb.echo.nasa.gov/reverb). This work was partially supported
by the Special Foundation for Free Exploration of State Laboratory of
Remote Sensing Science (Grant No. ZY12-11), the Natural Science Fund of
China (No. 41201331, No. 40901167 and No. 41101313), the High-Tech
Research and Development Program of China (No. 2009AA122100), the
Advance Research Program of Civil Aerospace Technology: Research on the
Key Techniques in Remote Sensing Data Processing for Solid Surface
Elements Extraction. J.B.F. contributed to this paper from the Jet
Propulsion Laboratory, California Institute of Technology, under a
contract with the National Aeronautics and Space Administration.
NR 80
TC 33
Z9 38
U1 4
U2 91
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0168-1923
EI 1873-2240
J9 AGR FOREST METEOROL
JI Agric. For. Meteorol.
PD APR 15
PY 2013
VL 171
BP 187
EP 202
DI 10.1016/j.agrformet.2012.11.016
PG 16
WC Agronomy; Forestry; Meteorology & Atmospheric Sciences
SC Agriculture; Forestry; Meteorology & Atmospheric Sciences
GA 111HS
UT WOS:000316513000018
ER
PT J
AU Derkowski, A
Bristow, TF
Wampler, JM
Srodon, J
Marynowski, L
Elliott, WC
Chamberlain, CP
AF Derkowski, Arkadiusz s
Bristow, Thomas F.
Wampler, J. M.
Srodon, Jan
Marynowski, Leszek
Elliott, W. Crawford
Chamberlain, C. Page
TI Hydrothermal alteration of the Ediacaran Doushantuo Formation in the
Yangtze Gorges area (South China)
SO GEOCHIMICA ET COSMOCHIMICA ACTA
LA English
DT Article
ID K-AR; ILLITE-SMECTITE; CLAY-MINERALS; NEOPROTEROZOIC DOUSHANTUO;
TRIOCTAHEDRAL SMECTITE; THERMAL MATURITY; LAYER SILICATES; DISTURBED
BELT; ROCK EXTRACTS; CAP CARBONATE
AB The geochemical and fossil record preserved in the Ediacaran age (635-551 Ma) Doushantuo Formation of South China has been extensively examined to explore the impact of changing climate and the oxidation state of the oceans on the development and distribution of early multicellular life. In the Yangtze Gorges area, this formation shows many of the geochemical trends and features thought to typify global ocean chemistry in the Ediacaran Period, but there are indications that post-sedimentary processes modified these signals. This study of clay minerals and organic matter builds a more detailed picture of the type and degree of post-sedimentary alteration at different stratigraphic levels of the formation and focuses on how this alteration influenced stable carbon and oxygen isotope records.
In the cratonward Jiulongwan and Huajipo sections of the Doushantuo Formation, its lower part (Members 1 and 2) consists largely of dolomitic shale, rich in authigenic saponite that crystallized in an alkaline sedimentary basin. Saponite has been altered to chlorite via corrensite across tens of meters of strata in lower Member 2, with increased alteration downward toward the cap dolostone. The greater chloritization is accompanied by lower delta O-18 and higher delta D values of trioctahedral clays. This pattern of alteration of trioctahedral clays is likely due to hydrothermal fluid activity in the underlying, relatively permeable Nantuo Formation and cap dolostone. A concomitant increase of solid bitumen reflectance toward the base of the formation supports this idea. In the uppermost part of the formation in the Yangtze Gorges area (Member 4), a typical open water marine dolomitic shale rich in illite and organic matter, increases in the methylphenanthrenes ratio index and solid bitumen reflectance correlate with decrease of the bulk rock K/Al ratio upward, providing evidence for hot fluid migration above the nearly impermeable shale.
Clay from the upper part of the formation is enriched in O-18, but not in D, relative to clay from the lower parts, indicating progressive O-18-enrichment of hydrothermal fluids that percolated upward and laterally through permeable O-18-rich carbonates. A maximum hydrothermal-alteration temperature of similar to 200 degrees C is estimated from a calibration curve for illitization during burial diagenesis, but given that the hydrothermal activity probably occurred in short pulses, the temperature could have been much higher. K-Ar ages are consistent across different size fractions of fine illite from Member 4 shale (similar to 430 Ma) and from a K-bentonite bed near the base of Member 2 in the Jiuqunao section (similar to 325 Ma), similar to 25 km from Jiulongwan and Huajipo. These age values show that the diagenetic illite of the Doushantuo Formation is a product of either deep burial diagenesis overprinted by spatially limited hydrothermal activity or of two localized hydrothermal events.
Patterns of carbonate C-13 and O-18 depletion in the basal Doushantuo Formation are similar to chloritization trends and O-18 variation in diagenetic clay minerals. Given independent evidence for C-13 depletion of hydrothermal fluids, these trends indicate carbonate-fluid isotope exchange commensurate with the degree of post-sedimentary alteration, supporting a model of lithologically controlled differential diagenesis induced by hydrothermal fluids as the main control on C and O isotope variability in this stratigraphic interval. This model could potentially explain other notable delta C-13 excursions higher up in Member 3. (C) 2013 Elsevier Ltd. All rights reserved.
C1 [Derkowski, Arkadiusz s; Srodon, Jan] Polish Acad Sci, Res Ctr Krakow, Inst Geol Sci, PL-31002 Krakow, Poland.
[Bristow, Thomas F.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Wampler, J. M.; Elliott, W. Crawford] Georgia State Univ, Dept Geosci, Atlanta, GA 30302 USA.
[Marynowski, Leszek] Univ Silesia, Fac Earth Sci, PL-41200 Sosnowiec, Poland.
[Chamberlain, C. Page] Stanford Univ, Dept Environm Earth Syst Sci, Stanford, CA 94305 USA.
RP Derkowski, A (reprint author), Polish Acad Sci, Res Ctr Krakow, Inst Geol Sci, Senacka 1, PL-31002 Krakow, Poland.
EM ndderkow@cyf-kr.edu.pl
NR 101
TC 15
Z9 15
U1 1
U2 74
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0016-7037
EI 1872-9533
J9 GEOCHIM COSMOCHIM AC
JI Geochim. Cosmochim. Acta
PD APR 15
PY 2013
VL 107
BP 279
EP 298
DI 10.1016/j.gca.2013.01.015
PG 20
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 100QA
UT WOS:000315714700019
ER
PT J
AU Keller, LP
Messenger, S
AF Keller, Lindsay P.
Messenger, Scott
TI On the origins of GEMS grains: A reply
SO GEOCHIMICA ET COSMOCHIMICA ACTA
LA English
DT Editorial Material
ID INTERPLANETARY DUST; MICROMETEORITES; ABUNDANCES; COMETS; STARS; IRON
AB The Comment by Bradley challenges our chemical and isotopic measurements of GEMS grains, arguing that pervasive infiltration of silicone oil and sample heating undermine our comparisons with equally uncertain interstellar grain compositions. However, we have already shown that such effects are negligible and cannot account for the extraordinary chemical variability of GEMS grains. Our data are also in excellent agreement with previous GEMS grain chemical analyses, and with GEMS grains in micrometeorites and within IDPs recently collected without the use of silicone oil. The order of magnitude variations in element abundances displayed by GEMS grains rule out a common origin by the extensive chemical and isotopic homogenization of circumstellar grains, as proposed by Bradley. The vast majority of GEMS grains also do not have radial compositional gradients, crystalline "relict" cores, or rims of condensed materials indicative of radiation exposure. The average element abundances of GEMS grains differ significantly and systematically from solar abundances and from those inferred for interstellar silicates based on element depletion patterns. A few GEMS grains have highly anomalous O isotopic compositions consistent with a condensation origin in evolved O-rich stellar envelopes and supernovae. Yet, on average, GEMS grains have O isotopic compositions very near to terrestrial and meteoritic values. These and other observations discussed in our paper place a strict upper limit on the number of GEMS grains that have preserved presolar origins. Published by Elsevier Ltd.
C1 [Keller, Lindsay P.; Messenger, Scott] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA.
RP Keller, LP (reprint author), NASA, Lyndon B Johnson Space Ctr, Mail Code KR,2101 NASA Pkwy, Houston, TX 77058 USA.
EM Lindsay.P.Keller@nasa.gov
NR 21
TC 8
Z9 8
U1 0
U2 8
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0016-7037
J9 GEOCHIM COSMOCHIM AC
JI Geochim. Cosmochim. Acta
PD APR 15
PY 2013
VL 107
BP 341
EP 344
DI 10.1016/j.gca.2012.11.012
PG 4
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 100QA
UT WOS:000315714700023
ER
PT J
AU Vazquez-Cuervo, J
Dewitte, B
Chin, TM
Armstrong, EM
Purca, S
Alburqueque, E
AF Vazquez-Cuervo, Jorge
Dewitte, Boris
Chin, Toshio M.
Armstrong, Edward M.
Purca, Sara
Alburqueque, Edward
TI An analysis of SST gradients off the Peruvian Coast: The impact of going
to higher resolution
SO REMOTE SENSING OF ENVIRONMENT
LA English
DT Article
DE Sea surface temperatures; Coastal/upwelling studies; Upwelling;
Satellite derived; Objective interpolation
ID SEA-SURFACE TEMPERATURE; CALIFORNIA CURRENT SYSTEM; PROJECT
AB The Peruvian Coastal Upwelling System (PCUS) is one of the most productive fisheries in the world. Upwelling events are associated with changes in the magnitude and location of frontal structures. SST gradients from four different data sets, NCDC, REMSS, OSTIA, and MUR are compared in two test areas off the PCUS: Paita (5 degrees S) and Pisco (14 degrees S). In both areas gradients derived from the MUR data set show greater magnitudes, as well as larger seasonal cycles. Off Pisco, the magnitude of the seasonal cycle of 2.2 degrees C/100 km in MUR is larger than the one derived from the lower resolution data sets. All data sets at Pisco exhibit a seasonal cycle that peaks in late Austral summer and early fall. Hovmoller diagrams calculated at 5.5 degrees S, 10.5 degrees S, and 14.5 degrees S show clearly defined offshore maxima in the cross-shore gradients for all the data sets. Upwelling scales determined by the distance to the first maxima vary depending on the data set used. At 5.5 degrees S upwelling scales vary from 10 km for MUR to 50 km for NCDC At 14.5 degrees S the scales vary from 20 km for MUR to 40 km for OSTIA. All four data sets show similar large-scale structures associated with the Peruvian upwelling. However, MUR shows finer scale structures that are most likely due to submesoscale to mesoscale eddies. Sub-sampled MUR 1 km data at the 25 km, 9 km, and 4 km resolutions compare well in magnitude and phase with the lower resolution products. Agreement in gradient magnitude between the lower resolution data sets and the MUR sub-sampled at their respective resolutions implies that the pixel-to-pixel analysis noise in MUR is at a similar level as the other data sets. (c) 2013 Elsevier Inc. All rights reserved.
C1 [Vazquez-Cuervo, Jorge; Chin, Toshio M.; Armstrong, Edward M.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Dewitte, Boris] IRD, LEGOS, Toulouse, France.
[Purca, Sara] Inst Mar Peru, Cello, Peru.
[Alburqueque, Edward] Univ Nacl Mayor San Marcos, Lima, Peru.
RP Vazquez-Cuervo, J (reprint author), CALTECH, Jet Prop Lab, M-S 300-323,4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM Jorge.Vazquez@jpl.nasa.gov
OI Purca, Sara/0000-0001-8751-1476
FU National Aeronautics and Space Administration at the Jet Propulsion
Laboratory, California Institute of Technology
FX The work was carried out under contract with the National Aeronautics
and Space Administration at the Jet Propulsion Laboratory, California
Institute of Technology. The authors gratefully thank Instituto del Mar
del Peru (IMARPE) for providing both scientific and technical support.
The authors also thank three anonymous reviewers for their hardwork and
thoughtful reviews in significantly improving this manuscript.
NR 32
TC 13
Z9 13
U1 2
U2 36
PU ELSEVIER SCIENCE INC
PI NEW YORK
PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA
SN 0034-4257
J9 REMOTE SENS ENVIRON
JI Remote Sens. Environ.
PD APR 15
PY 2013
VL 131
BP 76
EP 84
DI 10.1016/j.rse.2012.12.010
PG 9
WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic
Technology
SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science &
Photographic Technology
GA 098JZ
UT WOS:000315546900006
ER
PT J
AU Hassanin, AH
Said, MA
Seyam, AFM
AF Hassanin, Ahmed H.
Said, Magdi A.
Seyam, Abdel-Fattah M.
TI Composite Porous Membrane for Protecting High-Performance Fibers from
Ultraviolet-Visible Radiation
SO JOURNAL OF APPLIED POLYMER SCIENCE
LA English
DT Article
DE composites; degradation; membranes; nanoparticles; nanowires and
nanocrystals; radiation
ID P-PHENYLENEBENZOBISOXAZOLE FIBERS; TIO2 NANOPARTICLES; ARAMID FIBERS;
MECHANISMS
AB High-strength fibers are used to produce high-strength-to-weight-ratio materials for applications such as composites, soft and hard body armor, bulletproof vests, and tendons for scientific balloons. Unfortunately, these fibers degrade when they are exposed to ultraviolet-visible (UV-vis) radiation. The objective of this research was to develop systems to improve the UV resistance of such fibers. Composite porous membranes from a polyurethane (PU) matrix loaded with rutile titanium dioxide (TiO2) nanoparticles were developed to protect a braid made of polybenzobisoxazole (PBO) yarns. The PU membranes loaded with TiO2 nanoparticles were prepared by a phase-inversion technique. The effects of the amount of TiO2 nanoparticles on the composite membrane morphological structure and UV-vis light transmission were evaluated. The results show that when the concentration of TiO2 nanoparticles was increased, the porosity of the membrane and its UV-vis blocking effectiveness increased. The UV-vis protection was evaluated by the wrapping of the PBO braid with the composite membranes and exposed to UV-vis radiation. The strength loss of the PBO fiber due to exposure was decreased from 75% for the unprotected sample to 7.8% for the protected sample in the PU loaded with 4% TiO2 nanoparticles. (C) 2012 Wiley Periodicals, Inc. J. Appl. Polym. Sci. 128: 1297-1303, 2013
C1 [Hassanin, Ahmed H.; Seyam, Abdel-Fattah M.] N Carolina State Univ, Coll Text, Raleigh, NC 27695 USA.
[Said, Magdi A.] NASA, Wallops Flight Facil, Wallops Isl, VA 23337 USA.
RP Seyam, AFM (reprint author), N Carolina State Univ, Coll Text, Raleigh, NC 27695 USA.
EM aseyam@ncsu.edu
RI hassanin, ahmed/A-4718-2017
FU NASA, Balloon Research and Development Laboratory [NNXlOAE26G]
FX This work was funded by NASA, Balloon Research and Development
Laboratory (grant number NNXlOAE26G). The authors thank Rahul Vallabh of
North Carolina State University College of Textiles for his valuable
suggestions.
NR 18
TC 1
Z9 1
U1 2
U2 66
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 0021-8995
J9 J APPL POLYM SCI
JI J. Appl. Polym. Sci.
PD APR 15
PY 2013
VL 128
IS 2
SI SI
BP 1297
EP 1303
DI 10.1002/app.38476
PG 7
WC Polymer Science
SC Polymer Science
GA 089RD
UT WOS:000314926800049
ER
PT J
AU Bauschlicher, CW
Ricca, A
AF Bauschlicher, Charles W., Jr.
Ricca, Alessandra
TI On the calculation of the vibrational frequencies of C6H4
SO CHEMICAL PHYSICS LETTERS
LA English
DT Article
ID GAUSSIAN-BASIS SETS; ORTHO-BENZYNE; ELECTRON CORRELATION; ENERGY;
THERMOCHEMISTRY; APPROXIMATION; EXCHANGE
AB DFT and CCSD(T) frequencies are compared with experiment for ortho-benzyne (C6H4). Four bands are found to be in disagreement with experiment at the DFT level. Surprisingly the CCSD(T) method only brings the triple bond stretch into agreement with experiment, but leaves a sizable difference with experiment for the other three bands. The results for three isotopologues suggests that all of the differences cannot be attributed to resonances. Additional experimental work on ortho-benzyne appears warranted. Published by Elsevier B.V.
C1 [Bauschlicher, Charles W., Jr.] NASA, Ames Res Ctr, Space Technol Div, Moffett Field, CA 94035 USA.
[Ricca, Alessandra] SETI Inst, Mountain View, CA 94043 USA.
RP Bauschlicher, CW (reprint author), NASA, Ames Res Ctr, Space Technol Div, Mail Stop 230-3, Moffett Field, CA 94035 USA.
EM Charles.W.Bauschlicher@nasa.gov; Alessandra.Ricca-1@nasa.gov
FU NASA's Astronomy and Physics Research and Analysis (APRA) program
[NNX07AH02G]; Astrophysics Theory and Fundamental Physics (ATFP) program
[NNX09AD18G]
FX A.R. thank the NASA's Astronomy and Physics Research and Analysis (APRA)
(NNX07AH02G) and Astrophysics Theory and Fundamental Physics (ATFP)
(NNX09AD18G) programs for their generous support of this work.
NR 25
TC 2
Z9 2
U1 0
U2 14
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0009-2614
EI 1873-4448
J9 CHEM PHYS LETT
JI Chem. Phys. Lett.
PD APR 12
PY 2013
VL 566
BP 1
EP 3
DI 10.1016/j.cplett.2013.02.048
PG 3
WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical
SC Chemistry; Physics
GA 122WO
UT WOS:000317349300001
ER
PT J
AU Baker, DN
Kanekal, SG
Hoxie, VC
Henderson, MG
Li, X
Spence, HE
Elkington, SR
Friedel, RHW
Goldstein, J
Hudson, MK
Reeves, GD
Thorne, RM
Kletzing, CA
Claudepierre, SG
AF Baker, D. N.
Kanekal, S. G.
Hoxie, V. C.
Henderson, M. G.
Li, X.
Spence, H. E.
Elkington, S. R.
Friedel, R. H. W.
Goldstein, J.
Hudson, M. K.
Reeves, G. D.
Thorne, R. M.
Kletzing, C. A.
Claudepierre, S. G.
TI A Long-Lived Relativistic Electron Storage Ring Embedded in Earth's
Outer Van Allen Belt
SO SCIENCE
LA English
DT Article
ID RADIATION BELT; INNER MAGNETOSPHERE; CRRES; ACCELERATION; PROTONS;
MISSION; SAMPEX
AB Since their discovery more than 50 years ago, Earth's Van Allen radiation belts have been considered to consist of two distinct zones of trapped, highly energetic charged particles. The outer zone is composed predominantly of megaelectron volt (MeV) electrons that wax and wane in intensity on time scales ranging from hours to days, depending primarily on external forcing by the solar wind. The spatially separated inner zone is composed of commingled high-energy electrons and very energetic positive ions (mostly protons), the latter being stable in intensity levels over years to decades. In situ energy-specific and temporally resolved spacecraft observations reveal an isolated third ring, or torus, of high-energy (>2 MeV) electrons that formed on 2 September 2012 and persisted largely unchanged in the geocentric radial range of 3.0 to similar to 3.5 Earth radii for more than 4 weeks before being disrupted (and virtually annihilated) by a powerful interplanetary shock wave passage.
C1 [Baker, D. N.; Hoxie, V. C.; Li, X.; Elkington, S. R.] Univ Colorado, Lab Atmospher & Space Phys, Boulder, CO 80309 USA.
[Kanekal, S. G.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Henderson, M. G.; Friedel, R. H. W.; Reeves, G. D.] Los Alamos Natl Lab, Los Alamos, NM USA.
[Spence, H. E.] Univ New Hampshire, Inst Study Earth Oceans & Space, Durham, NH 03824 USA.
[Goldstein, J.] SW Res Inst, Space Sci & Engn Div, San Antonio, TX USA.
[Hudson, M. K.] Dartmouth Coll, Dept Phys & Astron, Hanover, NH 03755 USA.
[Thorne, R. M.] Univ Calif Los Angeles, Dept Atmospher & Ocean Sci, Los Angeles, CA USA.
[Kletzing, C. A.] Univ Iowa, Dept Phys & Astron, Iowa City, IA 52242 USA.
[Claudepierre, S. G.] Aerosp Corp, Los Angeles, CA 90009 USA.
RP Baker, DN (reprint author), Univ Colorado, Lab Atmospher & Space Phys, Boulder, CO 80309 USA.
EM daniel.baker@lasp.colorado.edu
RI Spence, Harlan/A-1942-2011; Friedel, Reiner/D-1410-2012; Henderson,
Michael/A-3948-2011;
OI Reeves, Geoffrey/0000-0002-7985-8098; Friedel,
Reiner/0000-0002-5228-0281; Henderson, Michael/0000-0003-4975-9029;
Kletzing, Craig/0000-0002-4136-3348; Spence, Harlan/0000-0002-2526-2205
FU RBSP-Energetic Particle Composition and Thermal Plasma Suite; Johns
Hopkins University Applied Physics Laboratory (JHU/APL) [967399,
921649]; NASA [NAS5-01072]
FX This work was supported by RBSP-Energetic Particle Composition and
Thermal Plasma Suite funding provided by the Johns Hopkins University
Applied Physics Laboratory (JHU/APL) contract no. 967399, Electric and
Magnetic Field Instrument Suite and Integrated Science (EMFISIS) work
was supported on JHU/APL contract no. 921649, and both were funded under
NASA's Prime contract no. NAS5-01072. All Van Allen Probes observations
used in this study, along with display and analysis software, are
publicly available at the Web site www.rbsp-ect.lanl.gov.
NR 26
TC 90
Z9 92
U1 1
U2 28
PU AMER ASSOC ADVANCEMENT SCIENCE
PI WASHINGTON
PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 USA
SN 0036-8075
EI 1095-9203
J9 SCIENCE
JI Science
PD APR 12
PY 2013
VL 340
IS 6129
BP 186
EP 190
DI 10.1126/science.1233518
PG 6
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 122TQ
UT WOS:000317341400053
PM 23450000
ER
PT J
AU Rury, AS
AF Rury, Aaron S.
TI Examining resonant inelastic spontaneous scattering of classical
Laguerre-Gauss beams from molecules
SO PHYSICAL REVIEW A
LA English
DT Article
ID RAY-EMISSION SPECTRA; RAMAN-SCATTERING; COHERENT CONTROL; LASER MODES;
INTERFERENCE; SPECTROSCOPY; DYNAMICS; EXCITATIONS; DIAMOND; LIGHT
AB This paper treats theoretically the spontaneous resonant inelastic scattering of Laguerre-Gauss (LG) beams from the vibrations of complex polyatomic molecules within the semiclassical framework. We develop an interaction Hamiltonian that accounts for the position of the molecule within the excitation beam to derive the effective differential scattering cross section of a classical LG beam from a molecule using the frequency-domain third-order nonlinear optical response function. To gain physical insight, we utilize a model vibronic molecule to study the changes to this scattering process. For specific molecular parameters including vibrational frequency and relative displacement of the involved electronic states, this investigation shows that an incident LG beam asymmetrically enhances one of two participating excitation transitions causing modulation of the interference present in the scattering process. This modulation allows a pathway to coherent control of resonant inelastic scattering from complex, polyatomic molecules. We discuss the possible application of this control to the resonant x-ray inelastic scattering (RIXS) of small polyatomic molecules central to applications ranging from single-molecule electronics to solar energy science. DOI: 10.1103/PhysRevA.87.043408
C1 [Rury, Aaron S.] Univ Michigan, Appl Phys Program, Ann Arbor, MI 48109 USA.
[Rury, Aaron S.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Rury, AS (reprint author), Univ Michigan, Appl Phys Program, Ann Arbor, MI 48109 USA.
EM arury@caltech.edu
OI Rury, Aaron/0000-0002-1836-1424
FU Defense Threat Reduction Agency-Joint Science and Technology Office for
Chemical and Biological Defense [HDTRA1-09-1-0005]
FX The author thanks R. J. Sension, P. R. Berman, D. G. Steel, and R. M.
Freeling for useful discussions. This work was supported by the Defense
Threat Reduction Agency-Joint Science and Technology Office for Chemical
and Biological Defense (Grant No. HDTRA1-09-1-0005).
NR 48
TC 7
Z9 7
U1 0
U2 16
PU AMER PHYSICAL SOC
PI COLLEGE PK
PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA
SN 1050-2947
J9 PHYS REV A
JI Phys. Rev. A
PD APR 11
PY 2013
VL 87
IS 4
AR 043408
DI 10.1103/PhysRevA.87.043408
PG 18
WC Optics; Physics, Atomic, Molecular & Chemical
SC Optics; Physics
GA 123KQ
UT WOS:000317388700006
ER
PT J
AU Kothadia, R
Kulecz, WB
Kofman, IS
Black, AJ
Grier, JW
Schlegel, TT
AF Kothadia, Roshni
Kulecz, Walter B.
Kofman, Igor S.
Black, Adam J.
Grier, James W.
Schlegel, Todd T.
TI New System for Digital to Analog Transformation and Reconstruction of
12-Lead ECGs
SO PLOS ONE
LA English
DT Article
ID COMPUTER-PROGRAMS; ELECTROCARDIOGRAMS; REPRODUCIBILITY; CONVERTERS;
DISEASE
AB Introduction: We describe initial validation of a new system for digital to analog conversion (DAC) and reconstruction of 12-lead ECGs. The system utilizes an open and optimized software format with a commensurately optimized DAC hardware configuration to accurately reproduce, from digital files, the original analog electrocardiographic signals of previously instrumented patients. By doing so, the system also ultimately allows for transmission of data collected on one manufacturer's 12-lead ECG hardware/software into that of any other.
Materials and Methods: To initially validate the system, we compared original and post-DAC re-digitized 12-lead ECG data files (similar to 5-minutes long) in two types of validation studies in 10 patients. The first type quantitatively compared the total waveform voltage differences between the original and re-digitized data while the second type qualitatively compared the automated electrocardiographic diagnostic statements generated by the original versus re-digitized data.
Results: The grand-averaged difference in root mean squared voltage between the original and re-digitized data was 20.8 mu V per channel when re-digitization involved the same manufacturer's analog to digital converter (ADC) as the original digitization, and 28.4 mu V per channel when it involved a different manufacturer's ADC. Automated diagnostic statements generated by the original versus reconstructed data did not differ when using the diagnostic algorithm from the same manufacturer on whose device the original data were collected, and differed only slightly for just 1 of 10 patients when using a third-party diagnostic algorithm throughout.
Conclusion: Original analog 12-lead ECG signals can be reconstructed from digital data files with accuracy sufficient for clinical use. Such reconstructions can readily enable automated second opinions for difficult-to-interpret 12-lead ECGs, either locally or remotely through the use of dedicated or cloud-based servers.
C1 [Kothadia, Roshni] Natl Space Biomed Res Inst, Houston, TX USA.
[Kulecz, Walter B.; Kofman, Igor S.] Wyle Sci Technol & Engn Grp, Houston, TX USA.
[Black, Adam J.] Univ Minnesota, Minneapolis, MN USA.
[Grier, James W.] N Dakota State Univ, Fargo, ND 58105 USA.
[Schlegel, Todd T.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA.
RP Schlegel, TT (reprint author), NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA.
EM todd.t.schlegel@nasa.gov
FU National Space Biomedical Research Institute summer student internship
program; NASA Johnson Space Center's Internal Research and Development
funds
FX Support for this work was provided by the National Space Biomedical
Research Institute summer student internship program (RK) and the NASA
Johnson Space Center's Internal Research and Development funds (TTS).
The funders had no role in study design, data collection and analysis,
decision to publish, or preparation of the manuscript.
NR 10
TC 2
Z9 2
U1 0
U2 4
PU PUBLIC LIBRARY SCIENCE
PI SAN FRANCISCO
PA 1160 BATTERY STREET, STE 100, SAN FRANCISCO, CA 94111 USA
SN 1932-6203
J9 PLOS ONE
JI PLoS One
PD APR 11
PY 2013
VL 8
IS 4
AR e61076
DI 10.1371/journal.pone.0061076
PG 10
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 123JA
UT WOS:000317383200040
PM 23613787
ER
PT J
AU Connerney, J
AF Connerney, Jack
TI SOLAR SYSTEM Saturn's ring rain
SO NATURE
LA English
DT Editorial Material
ID MODEL; IONOSPHERE; EVOLUTION
C1 NASA, Planetary Magnetospheres Lab, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Connerney, J (reprint author), NASA, Planetary Magnetospheres Lab, Goddard Space Flight Ctr, Code 695, Greenbelt, MD 20771 USA.
EM jack.connerney@nasa.gov
RI connerney, john/I-5127-2013;
OI connerney, jack/0000-0001-7478-6462
NR 18
TC 3
Z9 3
U1 1
U2 10
PU NATURE PUBLISHING GROUP
PI LONDON
PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND
SN 0028-0836
J9 NATURE
JI Nature
PD APR 11
PY 2013
VL 496
IS 7444
BP 178
EP 179
PG 2
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 122VM
UT WOS:000317346300032
PM 23579675
ER
PT J
AU O'Donoghue, J
Stallard, TS
Melin, H
Jones, GH
Cowley, SWH
Miller, S
Baines, KH
Blake, JSD
AF O'Donoghue, J.
Stallard, T. S.
Melin, H.
Jones, G. H.
Cowley, S. W. H.
Miller, S.
Baines, K. H.
Blake, J. S. D.
TI The domination of Saturn's low-latitude ionosphere by ring 'rain'
SO NATURE
LA English
DT Article
ID GIANT PLANET ATMOSPHERES; H-3(+); MODEL
AB Saturn's ionosphere is produced when the otherwise neutral atmosphere is exposed to a flow of energetic charged particles or solar radiation(1). At low latitudes the solar radiation should result in a weak planet-wide glow in the infrared, corresponding to the planet's uniform illumination by the Sun(2). The observed electron density of the low-latitude ionosphere, however, is lower and its temperature higher than predicted by models(3-5). A planet-to-ring magnetic connection has been previously suggested, in which an influx of water from the rings could explain the lower-than-expected electron densities in Saturn's atmosphere(6-8). Here we report the detection of a pattern of features, extending across a broad latitude band from 25 to 60 degrees, that is superposed on the lower-latitude background glow, with peaks in emission that map along the planet's magnetic field lines to gaps in Saturn's rings. This pattern implies the transfer of charged species derived from water from the ring-plane to the ionosphere, an influx on a global scale, flooding between 30 to 43 per cent of the surface of Saturn's upper atmosphere. This ring 'rain' is important in modulating ionospheric emissions and suppressing electron densities.
C1 [O'Donoghue, J.; Stallard, T. S.; Melin, H.; Cowley, S. W. H.; Blake, J. S. D.] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England.
[Jones, G. H.] Univ Coll London, Mullard Space Sci Lab, Dorking RH5 6NT, Surrey, England.
[Jones, G. H.; Miller, S.] Univ London Birkbeck Coll, Ctr Planetary Sci, London WC1E 6BT, England.
[Miller, S.] UCL, Dept Phys & Astron, Atmospher Phys Lab, London WC1E 6BT, England.
[Baines, K. H.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP O'Donoghue, J (reprint author), Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England.
EM jod3@ion.le.ac.uk
RI Jones, Geraint/C-1682-2008;
OI Stallard, Tom/0000-0003-3990-670X; Jones, Geraint/0000-0002-5859-1136;
O'Donoghue, James/0000-0002-4218-1191
FU UK Science and Technology Facilities Council (STFC)
FX The data presented here were obtained at the W. M. Keck Observatory,
which is operated as a scientific partnership among the California
Institute of Technology, the University of California and NASA. The
observations were made to support the Cassini auroral campaign. Ring
profile data were provided by the Planetary Rings Node
website18. Discussions within the international team led by
T. S. S. on 'Comparative Jovian Aeronomy' have greatly benefited this
work; this was hosted by the International Space Science Institute
(ISSI). The UK Science and Technology Facilities Council (STFC)
supported this work through the PhD Studentship of J.O'D. and grant
support for T. S. S., H. M. and G.H.J.
NR 18
TC 16
Z9 16
U1 1
U2 16
PU NATURE PUBLISHING GROUP
PI LONDON
PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND
SN 0028-0836
J9 NATURE
JI Nature
PD APR 11
PY 2013
VL 496
IS 7444
BP 193
EP 195
DI 10.1038/nature12049
PG 3
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 122VM
UT WOS:000317346300035
PM 23579676
ER
PT J
AU Bodnarik, JG
Burger, DM
Burger, A
Evans, LG
Parsons, AM
Schweitzer, JS
Starr, RD
Stassun, KG
AF Bodnarik, J. G.
Burger, D. M.
Burger, A.
Evans, L. G.
Parsons, A. M.
Schweitzer, J. S.
Starr, R. D.
Stassun, K. G.
TI Time-resolved neutron/gamma-ray data acquisition for in situ subsurface
planetary geochemistry
SO NUCLEAR INSTRUMENTS & METHODS IN PHYSICS RESEARCH SECTION A-ACCELERATORS
SPECTROMETERS DETECTORS AND ASSOCIATED EQUIPMENT
LA English
DT Article
DE Elemental analysis; Pulsed neutron generator; Time-tagged data
acquisition; Optimized time-gating; Time-dependent neutron and gamma-ray
detection
ID GAMMA-RAY; ACTIVE NEUTRON; SPECTROMETER; SURFACE; MARS
AB The current gamma-ray/neutron instrumentation development effort at NASA Goddard Space Flight Center aims to extend the use of active pulsed neutron interrogation techniques to probe the subsurface elemental composition of planetary bodies in situ. Previous NASA planetary science missions, that used neutron and/or gamma-ray spectroscopy instruments, have relied on neutrons produced from galactic cosmic rays. One of the distinguishing features of this effort is the inclusion of a high intensity 14.1 MeV pulsed neutron generator synchronized with a custom data acquisition system to time each event relative to the pulse. With usually only one opportunity to collect data, it is difficult to set a priori time-gating windows to obtain the best possible results. Acquiring time-tagged, event-by-event data from nuclear induced reactions provides raw data sets containing channel/energy, and event time for each gamma ray or neutron detected. The resulting data set can be plotted as a function of time or energy using optimized analysis windows after the data are acquired. Time windows can now be chosen to produce energy spectra that yield the most statistically significant and accurate elemental composition results that can be derived from the complete data set. The advantages of post-processing gamma-ray time-tagged event-by-event data in experimental tests using our prototype instrument will be demonstrated. Published by Elsevier B.V.
C1 [Bodnarik, J. G.; Parsons, A. M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Bodnarik, J. G.; Stassun, K. G.] Vanderbilt Univ, Dept Phys & Astron, Nashville, TN 37235 USA.
[Burger, D. M.] Vanderbilt Univ, Nashville, TN 37235 USA.
[Burger, A.] Fisk Univ, Dept Phys, Nashville, TN 37208 USA.
[Evans, L. G.] Comp Sci Corp, Lanham, MD 20706 USA.
[Schweitzer, J. S.] Univ Connecticut, Dept Phys, Storrs, CT 06269 USA.
[Starr, R. D.] Catholic Univ Amer, Inst Astrophys & Computat Sci, Washington, DC 20064 USA.
RP Bodnarik, JG (reprint author), NASA, Goddard Space Flight Ctr, 8800 Greenbelt Rd,Code 691, Greenbelt, MD 20771 USA.
EM julia.g.bodnarik@nasa.gov; dan.burger@vanderbilt.edu; aburger@fisk.edu;
larry.g.evans@nasa.gov; ann.m.parsons@nasa.gov; schweitz@phys.uconn.edu;
richard.d.starr@nasa.gov; keivan.stassun@vanderbilt.edu
FU NASA; NSF; Tennessee Space
FX We would like to thank S.L. Floyd, M. Namkung, and S.F. Nowicki for
assistance with acquiring the data. We would like to thank R. Forsythe
for assistance with the data analysis. We would like to thank J.I.
Trombka and T.P. McClanahan for many useful discussions. We are indebted
to NASA, NSF, and the Tennessee Space Grant for partial support of this
research.
NR 20
TC 9
Z9 9
U1 1
U2 23
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0168-9002
J9 NUCL INSTRUM METH A
JI Nucl. Instrum. Methods Phys. Res. Sect. A-Accel. Spectrom. Dect. Assoc.
Equip.
PD APR 11
PY 2013
VL 707
BP 135
EP 142
DI 10.1016/j.nima.2012.12.110
PG 8
WC Instruments & Instrumentation; Nuclear Science & Technology; Physics,
Nuclear; Physics, Particles & Fields
SC Instruments & Instrumentation; Nuclear Science & Technology; Physics
GA 090CI
UT WOS:000314956100020
ER
PT J
AU Aartsen, MG
Abbasi, R
Abdou, Y
Ackermann, M
Adams, J
Aguilar, JA
Ahlers, M
Altmann, D
Auffenberg, J
Bai, X
Baker, M
Barwick, SW
Baum, V
Bay, R
Beattie, K
Beatty, JJ
Bechet, S
Tjus, JB
Becker, KH
Bell, M
Benabderrahmane, ML
BenZvi, S
Berdermann, J
Berghaus, P
Berley, D
Bernardini, E
Bernhard, A
Bertrand, D
Besson, DZ
Bindig, D
Bissok, M
Blaufuss, E
Blumenthal, J
Boersma, DJ
Bohaichuk, S
Bohm, C
Bose, D
Boser, S
Botner, O
Brayeur, L
Brown, AM
Bruijn, R
Brunner, J
Buitink, S
Carson, M
Casey, J
Casier, M
Chirkin, D
Christy, B
Clark, K
Clevermann, F
Cohen, S
Cowen, DF
Silva, AHC
Danninger, M
Daughhetee, J
Davis, JC
De Clercq, C
De Ridder, S
Desiati, P
de Vries-Uiterweerd, G
de With, M
DeYoung, T
Diaz-Velez, JC
Dreyer, J
Dunkman, M
Eagan, R
Eberhardt, B
Eisch, J
Ellsworth, RW
Engdegard, O
Euler, S
Evenson, PA
Fadiran, O
Fazely, AR
Fedynitch, A
Feintzeig, J
Feusels, T
Filimonov, K
Finley, C
Fischer-Wasels, T
Flis, S
Franckowiak, A
Franke, R
Frantzen, K
Fuchs, T
Gaisser, TK
Gallagher, J
Gerhardt, L
Gladstone, L
Glusenkamp, T
Goldschmidt, A
Golup, G
Goodman, JA
Gora, D
Grant, D
Gross, A
Gurtner, M
Ha, C
Ismail, AH
Hallgren, A
Halzen, F
Hanson, K
Heereman, D
Heimann, P
Heinen, D
Helbing, K
Hellauer, R
Hickford, S
Hill, GC
Hoffman, KD
Hoffmann, R
Homeier, A
Hoshina, K
Huelsnitz, W
Hulth, PO
Hultqvist, K
Hussain, S
Ishihara, A
Jacobi, E
Jacobsen, J
Japaridze, GS
Jero, K
Jlelati, O
Kaminsky, B
Kappes, A
Karg, T
Karle, A
Kelley, JL
Kiryluk, J
Kislat, F
Klas, J
Klein, SR
Kohne, JH
Kohnen, G
Kolanoski, H
Kopke, L
Kopper, C
Kopper, S
Koskinen, DJ
Kowalski, M
Krasberg, M
Kroll, G
Kunnen, J
Kurahashi, N
Kuwabara, T
Labare, M
Landsman, H
Larson, MJ
Lesiak-Bzdak, M
Leute, J
Lunemann, J
Madsen, J
Maruyama, R
Mase, K
Matis, HS
McNally, F
Meagher, K
Merck, M
Meszaros, P
Meures, T
Miarecki, S
Middell, E
Milke, N
Miller, J
Mohrmann, L
Montaruli, T
Morse, R
Nahnhauer, R
Naumann, U
Niederhausen, H
Nowicki, SC
Nygren, DR
Obertacke, A
Odrowski, S
Olivas, A
Olivo, M
O'Murchadha, A
Panknin, S
Paul, L
Pepper, JA
de los Heros, CP
Pfendner, C
Pieloth, D
Pirk, N
Posselt, J
Price, PB
Przybylski, GT
Radel, L
Rawlins, K
Redl, P
Resconi, E
Rhode, W
Ribordy, M
Richman, M
Riedel, B
Rodrigues, JP
Rott, C
Ruhe, T
Ruzybayev, B
Ryckbosch, D
Saba, SM
Salameh, T
Sander, HG
Santander, M
Sarkar, S
Schatto, K
Scheel, M
Scheriau, F
Schmidt, T
Schmitz, M
Schoenen, S
Schoneberg, S
Schonherr, L
Schonwald, A
Schukraft, A
Schulte, L
Schulz, O
Seckel, D
Seo, SH
Sestayo, Y
Seunarine, S
Sheremata, C
Smith, MWE
Soiron, M
Soldin, D
Spiczak, GM
Spiering, C
Stamatikos, M
Stanev, T
Stasik, A
Stezelberger, T
Stokstad, RG
Stossl, A
Strahler, EA
Strom, R
Sullivan, GW
Taavola, H
Taboada, I
Tamburro, A
Ter-Antonyan, S
Tilav, S
Toale, PA
Toscano, S
Usner, M
van der Drift, D
van Eijndhoven, N
Van Overloop, A
van Santen, J
Vehring, M
Voge, M
Vraeghe, M
Walck, C
Waldenmaier, T
Wallraff, M
Wasserman, R
Weaver, C
Wellons, M
Wendt, C
Westerhoff, S
Whitehorn, N
Wiebe, K
Wiebusch, CH
Williams, DR
Wissing, H
Wolf, M
Wood, TR
Woschnagg, K
Xu, C
Xu, DL
Xu, XW
Yanez, JP
Yodh, G
Yoshida, S
Zarzhitsky, P
Ziemann, J
Zierke, S
Zilles, A
Zoll, M
AF Aartsen, M. G.
Abbasi, R.
Abdou, Y.
Ackermann, M.
Adams, J.
Aguilar, J. A.
Ahlers, M.
Altmann, D.
Auffenberg, J.
Bai, X.
Baker, M.
Barwick, S. W.
Baum, V.
Bay, R.
Beattie, K.
Beatty, J. J.
Bechet, S.
Tjus, J. Becker
Becker, K. -H.
Bell, M.
Benabderrahmane, M. L.
BenZvi, S.
Berdermann, J.
Berghaus, P.
Berley, D.
Bernardini, E.
Bernhard, A.
Bertrand, D.
Besson, D. Z.
Bindig, D.
Bissok, M.
Blaufuss, E.
Blumenthal, J.
Boersma, D. J.
Bohaichuk, S.
Bohm, C.
Bose, D.
Boeser, S.
Botner, O.
Brayeur, L.
Brown, A. M.
Bruijn, R.
Brunner, J.
Buitink, S.
Carson, M.
Casey, J.
Casier, M.
Chirkin, D.
Christy, B.
Clark, K.
Clevermann, F.
Cohen, S.
Cowen, D. F.
Silva, A. H. Cruz
Danninger, M.
Daughhetee, J.
Davis, J. C.
De Clercq, C.
De Ridder, S.
Desiati, P.
de Vries-Uiterweerd, G.
de With, M.
DeYoung, T.
Diaz-Velez, J. C.
Dreyer, J.
Dunkman, M.
Eagan, R.
Eberhardt, B.
Eisch, J.
Ellsworth, R. W.
Engdegard, O.
Euler, S.
Evenson, P. A.
Fadiran, O.
Fazely, A. R.
Fedynitch, A.
Feintzeig, J.
Feusels, T.
Filimonov, K.
Finley, C.
Fischer-Wasels, T.
Flis, S.
Franckowiak, A.
Franke, R.
Frantzen, K.
Fuchs, T.
Gaisser, T. K.
Gallagher, J.
Gerhardt, L.
Gladstone, L.
Gluesenkamp, T.
Goldschmidt, A.
Golup, G.
Goodman, J. A.
Gora, D.
Grant, D.
Gross, A.
Gurtner, M.
Ha, C.
Ismail, A. Haj
Hallgren, A.
Halzen, F.
Hanson, K.
Heereman, D.
Heimann, P.
Heinen, D.
Helbing, K.
Hellauer, R.
Hickford, S.
Hill, G. C.
Hoffman, K. D.
Hoffmann, R.
Homeier, A.
Hoshina, K.
Huelsnitz, W.
Hulth, P. O.
Hultqvist, K.
Hussain, S.
Ishihara, A.
Jacobi, E.
Jacobsen, J.
Japaridze, G. S.
Jero, K.
Jlelati, O.
Kaminsky, B.
Kappes, A.
Karg, T.
Karle, A.
Kelley, J. L.
Kiryluk, J.
Kislat, F.
Klaes, J.
Klein, S. R.
Koehne, J. -H.
Kohnen, G.
Kolanoski, H.
Koepke, L.
Kopper, C.
Kopper, S.
Koskinen, D. J.
Kowalski, M.
Krasberg, M.
Kroll, G.
Kunnen, J.
Kurahashi, N.
Kuwabara, T.
Labare, M.
Landsman, H.
Larson, M. J.
Lesiak-Bzdak, M.
Leute, J.
Luenemann, J.
Madsen, J.
Maruyama, R.
Mase, K.
Matis, H. S.
McNally, F.
Meagher, K.
Merck, M.
Meszaros, P.
Meures, T.
Miarecki, S.
Middell, E.
Milke, N.
Miller, J.
Mohrmann, L.
Montaruli, T.
Morse, R.
Nahnhauer, R.
Naumann, U.
Niederhausen, H.
Nowicki, S. C.
Nygren, D. R.
Obertacke, A.
Odrowski, S.
Olivas, A.
Olivo, M.
O'Murchadha, A.
Panknin, S.
Paul, L.
Pepper, J. A.
de los Heros, C. Perez
Pfendner, C.
Pieloth, D.
Pirk, N.
Posselt, J.
Price, P. B.
Przybylski, G. T.
Raedel, L.
Rawlins, K.
Redl, P.
Resconi, E.
Rhode, W.
Ribordy, M.
Richman, M.
Riedel, B.
Rodrigues, J. P.
Rott, C.
Ruhe, T.
Ruzybayev, B.
Ryckbosch, D.
Saba, S. M.
Salameh, T.
Sander, H. -G.
Santander, M.
Sarkar, S.
Schatto, K.
Scheel, M.
Scheriau, F.
Schmidt, T.
Schmitz, M.
Schoenen, S.
Schoeneberg, S.
Schoenherr, L.
Schoenwald, A.
Schukraft, A.
Schulte, L.
Schulz, O.
Seckel, D.
Seo, S. H.
Sestayo, Y.
Seunarine, S.
Sheremata, C.
Smith, M. W. E.
Soiron, M.
Soldin, D.
Spiczak, G. M.
Spiering, C.
Stamatikos, M.
Stanev, T.
Stasik, A.
Stezelberger, T.
Stokstad, R. G.
Stoessl, A.
Strahler, E. A.
Stroem, R.
Sullivan, G. W.
Taavola, H.
Taboada, I.
Tamburro, A.
Ter-Antonyan, S.
Tilav, S.
Toale, P. A.
Toscano, S.
Usner, M.
van der Drift, D.
van Eijndhoven, N.
Van Overloop, A.
van Santen, J.
Vehring, M.
Voge, M.
Vraeghe, M.
Walck, C.
Waldenmaier, T.
Wallraff, M.
Wasserman, R.
Weaver, Ch.
Wellons, M.
Wendt, C.
Westerhoff, S.
Whitehorn, N.
Wiebe, K.
Wiebusch, C. H.
Williams, D. R.
Wissing, H.
Wolf, M.
Wood, T. R.
Woschnagg, K.
Xu, C.
Xu, D. L.
Xu, X. W.
Yanez, J. P.
Yodh, G.
Yoshida, S.
Zarzhitsky, P.
Ziemann, J.
Zierke, S.
Zilles, A.
Zoll, M.
CA IceCube Collaboration
TI Measurement of the Atmospheric nu(e) Flux in IceCube
SO PHYSICAL REVIEW LETTERS
LA English
DT Article
ID NEUTRINO-INDUCED CASCADES; AMANDA; DETECTOR; DEEPCORE; SEARCH
AB We report the first measurement of the atmospheric electron neutrino flux in the energy range between approximately 80 GeV and 6 TeV, using data recorded during the first year of operation of IceCube's DeepCore low-energy extension. Techniques to identify neutrinos interacting within the DeepCore volume and veto muons originating outside the detector are demonstrated. A sample of 1029 events is observed in 281 days of data, of which 496 +/- 66(stat) +/- 88(syst) are estimated to be cascade events, including both electron neutrino and neutral current events. The rest of the sample includes residual backgrounds due to atmospheric muons and charged current interactions of atmospheric muon neutrinos. The flux of the atmospheric electron neutrinos is consistent with models of atmospheric neutrinos in this energy range. This constitutes the first observation of electron neutrinos and neutral current interactions in a very large volume neutrino telescope optimized for the TeV energy range. DOI: 10.1103/PhysRevLett.110.151105
C1 [Bissok, M.; Blumenthal, J.; Boersma, D. J.; Euler, S.; Heimann, P.; Heinen, D.; Paul, L.; Raedel, L.; Scheel, M.; Schoenen, S.; Schoenherr, L.; Schukraft, A.; Soiron, M.; Vehring, M.; Wallraff, M.; Wiebusch, C. H.; Zierke, S.; Zilles, A.] Rhein Westfal TH Aachen, Inst Phys 3, D-52056 Aachen, Germany.
[Aartsen, M. G.; Hill, G. C.] Univ Adelaide, Sch Chem & Phys, Adelaide, SA 5005, Australia.
[Rawlins, K.] Univ Alaska Anchorage, Dept Phys & Astron, Anchorage, AK 99508 USA.
[Japaridze, G. S.] Clark Atlanta Univ, CTSPS, Atlanta, GA 30314 USA.
[Casey, J.; Daughhetee, J.; Taboada, I.] Georgia Inst Technol, Sch Phys, Atlanta, GA 30332 USA.
[Casey, J.; Daughhetee, J.; Taboada, I.] Georgia Inst Technol, Ctr Relativist Astrophys, Atlanta, GA 30332 USA.
[Fazely, A. R.; Ter-Antonyan, S.; Xu, X. W.] Southern Univ, Dept Phys, Baton Rouge, LA 70813 USA.
[Bay, R.; Filimonov, K.; Gerhardt, L.; Ha, C.; Klein, S. R.; Miarecki, S.; Price, P. B.; van der Drift, D.; Woschnagg, K.] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA.
[Beattie, K.; Gerhardt, L.; Goldschmidt, A.; Ha, C.; Klein, S. R.; Matis, H. S.; Miarecki, S.; Nygren, D. R.; Przybylski, G. T.; Stezelberger, T.; Stokstad, R. G.; van der Drift, D.] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Berkeley, CA 94720 USA.
[Altmann, D.; de With, M.; Kappes, A.; Kolanoski, H.; Waldenmaier, T.] Humboldt Univ, Inst Phys, D-12489 Berlin, Germany.
[Tjus, J. Becker; Dreyer, J.; Fedynitch, A.; Olivo, M.; Saba, S. M.; Schoeneberg, S.] Ruhr Univ Bochum, Fac Phys & Astron, D-44780 Bochum, Germany.
[Boeser, S.; Franckowiak, A.; Homeier, A.; Kowalski, M.; Panknin, S.; Schulte, L.; Stasik, A.; Usner, M.; Voge, M.] Univ Bonn, Inst Phys, D-53115 Bonn, Germany.
[Bechet, S.; Bertrand, D.; Hanson, K.; Heereman, D.; Meures, T.; O'Murchadha, A.] Univ Libre Brussels, Fac Sci, B-1050 Brussels, Belgium.
[Bose, D.; Brayeur, L.; Buitink, S.; Casier, M.; De Clercq, C.; Golup, G.; Kunnen, J.; Labare, M.; Miller, J.; Strahler, E. A.; van Eijndhoven, N.] Vrije Univ Brussel, Dienst ELEM, B-1050 Brussels, Belgium.
[Ishihara, A.; Mase, K.; Yoshida, S.] Chiba Univ, Dept Phys, Chiba 2638522, Japan.
[Adams, J.; Brown, A. M.; Hickford, S.] Univ Canterbury, Dept Phys & Astron, Christchurch 1, New Zealand.
[Berley, D.; Blaufuss, E.; Christy, B.; Ellsworth, R. W.; Goodman, J. A.; Hellauer, R.; Hoffman, K. D.; Huelsnitz, W.; Meagher, K.; Olivas, A.; Redl, P.; Richman, M.; Schmidt, T.; Sullivan, G. W.; Wissing, H.] Univ Maryland, Dept Phys, College Pk, MD 20742 USA.
[Beatty, J. J.; Davis, J. C.; Pfendner, C.; Rott, C.; Stamatikos, M.] Ohio State Univ, Dept Phys, Columbus, OH 43210 USA.
[Beatty, J. J.; Davis, J. C.; Pfendner, C.; Rott, C.; Stamatikos, M.] Ohio State Univ, Ctr Cosmol & Astroparticle Phys, Columbus, OH 43210 USA.
[Beatty, J. J.] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA.
[Clevermann, F.; Frantzen, K.; Fuchs, T.; Koehne, J. -H.; Milke, N.; Pieloth, D.; Rhode, W.; Ruhe, T.; Scheriau, F.; Schmitz, M.; Ziemann, J.] TU Dortmund Univ, Dept Phys, D-44221 Dortmund, Germany.
[Bohaichuk, S.; Grant, D.; Nowicki, S. C.; Sheremata, C.; Wood, T. R.] Univ Alberta, Dept Phys, Edmonton, AB T6G 2G7, Canada.
[Aguilar, J. A.; Montaruli, T.] Univ Geneva, Dept Phys Nucl & Corpusculaire, CH-1211 Geneva, Switzerland.
[Abdou, Y.; Carson, M.; De Ridder, S.; de Vries-Uiterweerd, G.; Feusels, T.; Ismail, A. Haj; Jlelati, O.; Ryckbosch, D.; Van Overloop, A.; Vraeghe, M.] Univ Ghent, Dept Phys & Astron, B-9000 Ghent, Belgium.
[Barwick, S. W.; Yodh, G.] Univ Calif Irvine, Dept Phys & Astron, Irvine, CA 92697 USA.
[Bruijn, R.; Cohen, S.; Ribordy, M.] Ecole Polytech Fed Lausanne, High Energy Phys Lab, CH-1015 Lausanne, Switzerland.
[Besson, D. Z.] Univ Kansas, Dept Phys & Astron, Lawrence, KS 66045 USA.
[Gallagher, J.] Univ Wisconsin, Dept Astron, Madison, WI 53706 USA.
[Abbasi, R.; Ahlers, M.; Auffenberg, J.; Baker, M.; BenZvi, S.; Chirkin, D.; Desiati, P.; Diaz-Velez, J. C.; Eisch, J.; Fadiran, O.; Feintzeig, J.; Gladstone, L.; Halzen, F.; Hoshina, K.; Jacobsen, J.; Jero, K.; Karle, A.; Kelley, J. L.; Koepke, L.; Kopper, C.; Krasberg, M.; Kurahashi, N.; Landsman, H.; Maruyama, R.; McNally, F.; Merck, M.; Morse, R.; Riedel, B.; Rodrigues, J. P.; Santander, M.; Toscano, S.; van Santen, J.; Weaver, Ch.; Wellons, M.; Wendt, C.; Westerhoff, S.; Whitehorn, N.] Univ Wisconsin, Dept Phys, Madison, WI 53706 USA.
[Abbasi, R.; Ahlers, M.; Auffenberg, J.; Baker, M.; BenZvi, S.; Chirkin, D.; Desiati, P.; Diaz-Velez, J. C.; Eisch, J.; Fadiran, O.; Feintzeig, J.; Gladstone, L.; Halzen, F.; Hoshina, K.; Jacobsen, J.; Jero, K.; Karle, A.; Kelley, J. L.; Koepke, L.; Kopper, C.; Krasberg, M.; Kurahashi, N.; Landsman, H.; Maruyama, R.; McNally, F.; Merck, M.; Morse, R.; Riedel, B.; Rodrigues, J. P.; Santander, M.; Toscano, S.; van Santen, J.; Weaver, Ch.; Wellons, M.; Wendt, C.; Westerhoff, S.; Whitehorn, N.] Univ Wisconsin, Wisconsin IceCube Particle Astrophys Ctr, Madison, WI 53706 USA.
[Baum, V.; Eberhardt, B.; Kroll, G.; Luenemann, J.; Sander, H. -G.; Schatto, K.; Wiebe, K.] Johannes Gutenberg Univ Mainz, Inst Phys, D-55099 Mainz, Germany.
[Kohnen, G.] Univ Mons, B-7000 Mons, Belgium.
[Bernhard, A.; Gross, A.; Leute, J.; Odrowski, S.; Resconi, E.; Schulz, O.; Sestayo, Y.] Tech Univ Munich, D-85748 Garching, Germany.
[Bai, X.; Evenson, P. A.; Gaisser, T. K.; Hussain, S.; Kuwabara, T.; Ruzybayev, B.; Seckel, D.; Stanev, T.; Tamburro, A.; Tilav, S.; Xu, C.] Univ Delaware, Bartol Res Inst, Newark, DE 19716 USA.
[Bai, X.; Evenson, P. A.; Gaisser, T. K.; Hussain, S.; Kuwabara, T.; Ruzybayev, B.; Seckel, D.; Stanev, T.; Tamburro, A.; Tilav, S.; Xu, C.] Univ Delaware, Dept Phys & Astron, Newark, DE 19716 USA.
[Sarkar, S.] Univ Oxford, Dept Phys, Oxford OX1 3NP, England.
[Madsen, J.; Seunarine, S.; Spiczak, G. M.] Univ Wisconsin, Dept Phys, River Falls, WI 54022 USA.
[Bohm, C.; Danninger, M.; Finley, C.; Flis, S.; Hulth, P. O.; Hultqvist, K.; Seo, S. H.; Walck, C.; Wolf, M.; Zoll, M.] Stockholm Univ, Oskar Klein Ctr, SE-10691 Stockholm, Sweden.
[Bohm, C.; Danninger, M.; Finley, C.; Flis, S.; Hulth, P. O.; Hultqvist, K.; Seo, S. H.; Walck, C.; Wolf, M.; Zoll, M.] Stockholm Univ, Dept Phys, SE-10691 Stockholm, Sweden.
[Kiryluk, J.; Lesiak-Bzdak, M.; Niederhausen, H.] SUNY Stony Brook, Dept Phys & Astron, Stony Brook, NY 11794 USA.
[Larson, M. J.; Pepper, J. A.; Toale, P. A.; Williams, D. R.; Xu, D. L.; Zarzhitsky, P.] Univ Alabama, Dept Phys & Astron, Tuscaloosa, AL 35487 USA.
[Cowen, D. F.; Meszaros, P.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA.
[Bell, M.; Clark, K.; Cowen, D. F.; DeYoung, T.; Dunkman, M.; Eagan, R.; Koskinen, D. J.; Meszaros, P.; Salameh, T.; Smith, M. W. E.; Wasserman, R.] Penn State Univ, Dept Phys, University Pk, PA 16802 USA.
[Boersma, D. J.; Botner, O.; Engdegard, O.; Hallgren, A.; de los Heros, C. Perez; Stroem, R.; Taavola, H.] Uppsala Univ, Dept Phys & Astron, S-75120 Uppsala, Sweden.
[Becker, K. -H.; Bindig, D.; Fischer-Wasels, T.; Gurtner, M.; Helbing, K.; Hoffmann, R.; Klaes, J.; Kopper, S.; Naumann, U.; Obertacke, A.; Posselt, J.; Soldin, D.] Berg Univ Wuppertal, Dept Phys, D-42119 Wuppertal, Germany.
[Ackermann, M.; Benabderrahmane, M. L.; Berdermann, J.; Berghaus, P.; Bernardini, E.; Brunner, J.; Silva, A. H. Cruz; Franke, R.; Gluesenkamp, T.; Gora, D.; Jacobi, E.; Kaminsky, B.; Karg, T.; Kislat, F.; Middell, E.; Mohrmann, L.; Nahnhauer, R.; Pirk, N.; Schoenwald, A.; Spiering, C.; Stoessl, A.; Yanez, J. P.] DESY, D-15735 Zeuthen, Germany.
[Bai, X.] South Dakota Sch Mines & Technol, Dept Phys, Rapid City, SD 57701 USA.
[Huelsnitz, W.] Los Alamos Natl Lab, Los Alamos, NM 87545 USA.
[Montaruli, T.] Dipartimento Fis, Sez INFN, I-70126 Bari, Italy.
[Stamatikos, M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP DeYoung, T (reprint author), Penn State Univ, Dept Phys, 104 Davey Lab, University Pk, PA 16802 USA.
RI Tjus, Julia/G-8145-2012; Wiebusch, Christopher/G-6490-2012; Auffenberg,
Jan/D-3954-2014; Koskinen, David/G-3236-2014; Brunner,
Juergen/G-3540-2015; Aguilar Sanchez, Juan Antonio/H-4467-2015;
Maruyama, Reina/A-1064-2013; Sarkar, Subir/G-5978-2011; Beatty,
James/D-9310-2011;
OI Schukraft, Anne/0000-0002-9112-5479; Wiebusch,
Christopher/0000-0002-6418-3008; Auffenberg, Jan/0000-0002-1185-9094;
Koskinen, David/0000-0002-0514-5917; Brunner,
Juergen/0000-0002-5052-7236; Aguilar Sanchez, Juan
Antonio/0000-0003-2252-9514; Maruyama, Reina/0000-0003-2794-512X;
Sarkar, Subir/0000-0002-3542-858X; Beatty, James/0000-0003-0481-4952;
Ter-Antonyan, Samvel/0000-0002-5788-1369
FU U.S. National Science Foundation-Office of Polar Programs; U.S. National
Science Foundation-Physics Division; University of Wisconsin Alumni
Research Foundation; Grid Laboratory Of Wisconsin (GLOW) grid
infrastructure at the University of Wisconsin-Madison; Open Science Grid
(OSG) grid infrastructure; U.S. Department of Energy; National Energy
Research Scientific Computing Center; Louisiana Optical Network
Initiative (LONI) grid computing resources; National Science and
Engineering Research Council of Canada; Swedish Research Council;
Swedish Polar Research Secretariat; Swedish National Infrastructure for
Computing (SNIC); Knut and Alice Wallenberg Foundation, Sweden; German
Ministry for Education and Research (BMBF); Deutsche
Forschungsgemeinschaft (DFG); Helmholtz Alliance for Astroparticle
Physics (HAP); Research Department of Plasmas with Complex Interactions
(Bochum), Germany; Fund for Scientific Research (FNRS-FWO); FWO Odysseus
programme; Flanders Institute to encourage scientific and technological
research in industry (IWT); Belgian Federal Science Policy Office
(Belspo); University of Oxford, U.K.; Marsden Fund, New Zealand;
Australian Research Council; Japan Society for Promotion of Science
(JSPS); Swiss National Science Foundation (SNSF), Switzerland
FX We acknowledge the support from the following agencies: U.S. National
Science Foundation-Office of Polar Programs, U.S. National Science
Foundation-Physics Division, University of Wisconsin Alumni Research
Foundation, the Grid Laboratory Of Wisconsin (GLOW) grid infrastructure
at the University of Wisconsin-Madison, the Open Science Grid (OSG) grid
infrastructure; U.S. Department of Energy, and National Energy Research
Scientific Computing Center, the Louisiana Optical Network Initiative
(LONI) grid computing resources; National Science and Engineering
Research Council of Canada; Swedish Research Council, Swedish Polar
Research Secretariat, Swedish National Infrastructure for Computing
(SNIC), and Knut and Alice Wallenberg Foundation, Sweden; German
Ministry for Education and Research (BMBF), Deutsche
Forschungsgemeinschaft (DFG), Helmholtz Alliance for Astroparticle
Physics (HAP), Research Department of Plasmas with Complex Interactions
(Bochum), Germany; Fund for Scientific Research (FNRS-FWO), FWO Odysseus
programme, Flanders Institute to encourage scientific and technological
research in industry (IWT), Belgian Federal Science Policy Office
(Belspo); University of Oxford, U.K.; Marsden Fund, New Zealand;
Australian Research Council; Japan Society for Promotion of Science
(JSPS); the Swiss National Science Foundation (SNSF), Switzerland.
NR 33
TC 38
Z9 38
U1 0
U2 13
PU AMER PHYSICAL SOC
PI COLLEGE PK
PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA
SN 0031-9007
J9 PHYS REV LETT
JI Phys. Rev. Lett.
PD APR 10
PY 2013
VL 110
IS 15
AR 151105
DI 10.1103/PhysRevLett.110.151105
PG 7
WC Physics, Multidisciplinary
SC Physics
GA 124JJ
UT WOS:000317459300004
PM 25167245
ER
PT J
AU Metaferia, B
Wei, JS
Song, YK
Evangelista, J
Aschenbach, K
Johansson, P
Wen, XY
Chen, QR
Lee, A
Hempel, H
Gheeya, JS
Getty, S
Gomez, R
Khan, J
AF Metaferia, Belhu
Wei, Jun S.
Song, Young K.
Evangelista, Jennifer
Aschenbach, Konrad
Johansson, Peter
Wen, Xinyu
Chen, Qingrong
Lee, Albert
Hempel, Heidi
Gheeya, Jinesh S.
Getty, Stephanie
Gomez, Romel
Khan, Javed
TI Development of Peptide Nucleic Acid Probes for Detection of the HER2
Oncogene
SO PLOS ONE
LA English
DT Article
ID BREAST-CANCER; HYBRIDIZATION; PNA; DNA; IMMOBILIZATION; RESISTANCE;
STABILITY; PNA/DNA; CELLS; RNA
AB Peptide nucleic acids (PNAs) have gained much interest as molecular recognition tools in biology, medicine and chemistry. This is due to high hybridization efficiency to complimentary oligonucleotides and stability of the duplexes with RNA or DNA. We have synthesized 15/16-mer PNA probes to detect the HER2 mRNA. The performance of these probes to detect the HER2 target was evaluated by fluorescence imaging and fluorescence bead assays. The PNA probes have sufficiently discriminated between the wild type HER2 target and the mutant target with single base mismatches. Furthermore, the probes exhibited excellent linear concentration dependence between 0.4 to 400 fmol for the target gene. The results demonstrate potential application of PNAs as diagnostic probes with high specificity for quantitative measurements of amplifications or over-expressions of oncogenes.
C1 [Metaferia, Belhu; Wei, Jun S.; Song, Young K.; Johansson, Peter; Wen, Xinyu; Chen, Qingrong; Lee, Albert; Hempel, Heidi; Gheeya, Jinesh S.; Khan, Javed] NCI, Pediat Oncol Branch, NIH, Bethesda, MD 20892 USA.
[Wen, Xinyu] NCI, Adv Biomed Comp Ctr, SAIC Frederick Inc, Frederick, MD 21701 USA.
[Evangelista, Jennifer; Aschenbach, Konrad; Gomez, Romel] Univ Maryland, Dept Elect & Comp Engn, College Pk, MD 20742 USA.
[Getty, Stephanie] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Khan, J (reprint author), NCI, Pediat Oncol Branch, NIH, Bethesda, MD 20892 USA.
EM khanjav@mail.nih.gov
RI Getty, Stephanie/D-7037-2012; Khan, Javed/P-9157-2014; Johansson,
Peter/K-1053-2014;
OI Khan, Javed/0000-0002-5858-0488; Johansson, Peter/0000-0001-7015-5452;
Gheeya, Jinesh/0000-0002-5246-6262
FU National Institutes of Health, National Cancer Institute, Center for
Cancer Research
FX This study was supported by the Intramural Research Program of the
National Institutes of Health, National Cancer Institute, Center for
Cancer Research. The funders had no role in study design, data
collection and analysis, decision to publish, or preparation of the
manuscript.
NR 31
TC 1
Z9 1
U1 0
U2 31
PU PUBLIC LIBRARY SCIENCE
PI SAN FRANCISCO
PA 1160 BATTERY STREET, STE 100, SAN FRANCISCO, CA 94111 USA
SN 1932-6203
J9 PLOS ONE
JI PLoS One
PD APR 10
PY 2013
VL 8
IS 4
AR e58870
DI 10.1371/journal.pone.0058870
PG 7
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 123IQ
UT WOS:000317382000002
PM 23593123
ER
PT J
AU Follette, KB
Tamura, M
Hashimoto, J
Whitney, B
Grady, C
Close, L
Andrews, SM
Kwon, J
Wisniewski, J
Brandt, TD
Mayama, S
Kandori, R
Dong, RB
Abe, L
Brandner, W
Carson, J
Currie, T
Egner, SE
Feldt, M
Goto, M
Guyon, O
Hayano, Y
Hayashi, M
Hayashi, S
Henning, T
Hodapp, K
Ishii, M
Iye, M
Janson, M
Knapp, GR
Kudo, T
Kusakabe, N
Kuzuhara, M
McElwain, MW
Matsuo, T
Miyama, S
Morino, JI
Moro-Martin, A
Nishimura, T
Pyo, TS
Serabyn, E
Suto, H
Suzuki, R
Takami, M
Takato, N
Terada, H
Thalmann, C
Tomono, D
Turner, EL
Watanabe, M
Yamada, T
Takami, H
Usuda, T
AF Follette, Katherine B.
Tamura, Motohide
Hashimoto, Jun
Whitney, Barbara
Grady, Carol
Close, Laird
Andrews, Sean M.
Kwon, Jungmi
Wisniewski, John
Brandt, Timothy D.
Mayama, Satoshi
Kandori, Ryo
Dong, Ruobing
Abe, Lyu
Brandner, Wolfgang
Carson, Joseph
Currie, Thayne
Egner, Sebastian E.
Feldt, Markus
Goto, Miwa
Guyon, Olivier
Hayano, Yutaka
Hayashi, Masahiko
Hayashi, Saeko
Henning, Thomas
Hodapp, Klaus
Ishii, Miki
Iye, Masanori
Janson, Markus
Knapp, Gillian R.
Kudo, Tomoyuki
Kusakabe, Nobuhiko
Kuzuhara, Masayuki
McElwain, Michael W.
Matsuo, Taro
Miyama, Shoken
Morino, Jun-Ichi
Moro-Martin, Amaya
Nishimura, Tetsuo
Pyo, Tae-Soo
Serabyn, Eugene
Suto, Hiroshi
Suzuki, Ryuji
Takami, Michihiro
Takato, Naruhisa
Terada, Hiroshi
Thalmann, Christian
Tomono, Daigo
Turner, Edwin L.
Watanabe, Makoto
Yamada, Toru
Takami, Hideki
Usuda, Tomonori
TI MAPPING H-BAND SCATTERED LIGHT EMISSION IN THE MYSTERIOUS SR21
TRANSITIONAL DISK
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE planetary systems; protoplanetary disks; stars: individual (SR21);
stars: pre-main sequence; techniques: polarimetric
ID MAIN-SEQUENCE STARS; 2-DIMENSIONAL RADIATIVE-TRANSFER; YOUNG STELLAR
OBJECTS; PROTOPLANETARY DISKS; CIRCUMSTELLAR DUST; PROTOSTELLAR
ENVELOPES; SIZE DISTRIBUTION; MOLECULAR CLOUD; FORMING REGION; GIANT
PLANETS
AB We present the first near infrared (NIR) spatially resolved images of the circumstellar transitional disk around SR21. These images were obtained with the Subaru HiCIAO camera, adaptive optics, and the polarized differential imaging technique. We resolve the disk in scattered light at H-band for stellocentric 0 ''.1 <= r <= 0 ''.6 (12 less than or similar to r less than or similar to 75 AU). We compare our results with previously published spatially resolved 880 mu m continuum Submillimeter Array images that show an inner r less than or similar to 36 AU cavity in SR21. Radiative transfer models reveal that the large disk depletion factor invoked to explain SR21's sub-mm cavity cannot be "universal" for all grain sizes. Even significantly more moderate depletions (delta = 0.1, 0.01 relative to an undepleted disk) than those that reproduce the sub-mm cavity (delta similar to 10(-6)) are inconsistent with our H-band images when they are assumed to carry over to small grains, suggesting that surface grains scattering in the NIR either survive or are generated by whatever mechanism is clearing the disk midplane. In fact, the radial polarized intensity profile of our H-band observations is smooth and steeply inwardly-increasing (r(-3)), with no evidence of a break at the 36 AU sub-mm cavity wall. We hypothesize that this profile is dominated by an optically thin disk envelope or atmosphere component. We also discuss the compatibility of our data with the previously postulated existence of a sub-stellar companion to SR21 at r similar to 10-20 AU, and find that we can neither exclude nor verify this scenario. This study demonstrates the power of multiwavelength imaging of transitional disks to inform modeling efforts, including the debate over precisely what physical mechanism is responsible for clearing these disks of their large midplane grains.
C1 [Follette, Katherine B.; Close, Laird] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA.
[Tamura, Motohide; Hashimoto, Jun; Kwon, Jungmi; Kandori, Ryo; Iye, Masanori; Kusakabe, Nobuhiko; Kuzuhara, Masayuki; Morino, Jun-Ichi; Suto, Hiroshi] Natl Astron Observ Japan, Mitaka, Tokyo 1818588, Japan.
[Tamura, Motohide; Kwon, Jungmi] Grad Univ Adv Studies Sokendai, Dept Astron Sci, Tokyo 1818588, Japan.
[Whitney, Barbara] Univ Wisconsin, Dept Astron, Madison, WI 53706 USA.
[Grady, Carol] Eureka Sci, Oakland, CA 96002 USA.
[Andrews, Sean M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Wisniewski, John] Univ Oklahoma, HL Dodge Dept Phys & Astron, Norman, OK 73019 USA.
[Brandt, Timothy D.; Dong, Ruobing; Janson, Markus; Knapp, Gillian R.; Turner, Edwin L.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA.
[Mayama, Satoshi] Grad Univ Adv Studies Sokendai, Ctr Promot Integrated Sci, Hayama, Kanagawa 2400193, Japan.
[Abe, Lyu] Univ Nice Sophia Antipolis, CNRS, Observ Cote Azur, Lab Lagrange,UMR7293, F-06300 Nice, France.
[Brandner, Wolfgang; Feldt, Markus; Henning, Thomas] Max Planck Inst Astron, D-69117 Heidelberg, Germany.
[Carson, Joseph] Coll Charleston, Dept Phys & Astron, Charleston, SC 29424 USA.
[Currie, Thayne] Univ Toronto, Dept Astron & Astrophys, Toronto, ON M5S 3H4, Canada.
[Egner, Sebastian E.; Guyon, Olivier; Hayano, Yutaka; Hayashi, Saeko; Ishii, Miki; Kudo, Tomoyuki; Nishimura, Tetsuo; Pyo, Tae-Soo; Takato, Naruhisa; Terada, Hiroshi; Tomono, Daigo; Takami, Hideki; Usuda, Tomonori] Subaru Telescope, Hilo, HI 96720 USA.
[Goto, Miwa] Univ Munich, Univ Sternwarte Munchen, D-81679 Munich, Germany.
[Hayashi, Masahiko] Univ Tokyo, Dept Astron, Bunkyo Ku, Tokyo 1130033, Japan.
[Hodapp, Klaus] Univ Hawaii, Inst Astron, Hilo, HI 96720 USA.
[McElwain, Michael W.] NASA, Goddard Space Flight Ctr, ExoPlanets & Stellar Astrophys Lab, Greenbelt, MD 20771 USA.
[Matsuo, Taro] Kyoto Univ, Dept Astron, Sakyo Ku, Kitashirakawa Oiwake, Kyoto 6068502, Japan.
[Miyama, Shoken] Hiroshima Univ, Off President, Higashihiroshima 7398511, Japan.
[Moro-Martin, Amaya] Inst Nacl Tecn Aeroespacial, CAB INTA CSIC, Dept Astrofis, E-28850 Madrid, Spain.
[Serabyn, Eugene] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Suzuki, Ryuji] TMT Observ Corp, Pasadena, CA 91105 USA.
[Takami, Michihiro] Acad Sinica, Inst Astron & Astrophys, Taipei 106, Taiwan.
[Thalmann, Christian] Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1098 XH Amsterdam, Netherlands.
[Turner, Edwin L.] Univ Tokyo, Kavli Inst Phys & Math Universe, Kashiwa, Chiba 2778568, Japan.
[Watanabe, Makoto] Hokkaido Univ, Dept Cosmosci, Sapporo, Hokkaido 0600810, Japan.
[Yamada, Toru] Tohoku Univ, Astron Inst, Aoba Ku, Sendai, Miyagi 9808578, Japan.
RP Follette, KB (reprint author), Univ Arizona, Steward Observ, 933 N Cherry Ave, Tucson, AZ 85721 USA.
EM kfollette@as.arizona.edu
RI MIYAMA, Shoken/A-3598-2015; Watanabe, Makoto/E-3667-2016
OI Watanabe, Makoto/0000-0002-3656-4081
FU National Science Foundation; MEXT; [NSF-AST 1009314]; [NSF-AST
1009203]
FX We gratefully acknowledge funding from the National Science Foundation
East Asian and Pacific Summer Institute Fellowship (Follette), NSF-AST
1009314 (Wisniewski) and NSF-AST 1009203 (Carson). We are grateful to
Collette Salyk, Glenn Schneider, Dean Hines, Don McCarthy, Vanessa
Bailey, and Johanna Teske for their insightful comments. The authors
wish to recognize and acknowledge the very significant cultural role and
reverence that the summit of Mauna Kea has always had within the
indigenous Hawaiian community. We are most fortunate to have the
opportunity to conduct observations from this mountain. Part of this
work was carried out at JPL. This work is partly supported by a
Grant-in-Aid for Science Research in a Priority Area from MEXT.
NR 77
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PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD APR 10
PY 2013
VL 767
IS 1
AR 10
DI 10.1088/0004-637X/767/1/10
PG 26
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 117IT
UT WOS:000316947500010
ER
PT J
AU Guyon, O
Eisner, JA
Angel, R
Woolf, NJ
Bendek, EA
Milster, TD
Ammons, SM
Shao, M
Shaklan, S
Levine, M
Nemati, B
Martinache, F
Pitman, J
Woodruff, RA
Belikov, R
AF Guyon, Olivier
Eisner, Josh A.
Angel, Roger
Woolf, Neville J.
Bendek, Eduardo A.
Milster, Thomas D.
Ammons, S. Mark
Shao, Michael
Shaklan, Stuart
Levine, Marie
Nemati, Bijan
Martinache, Frantz
Pitman, Joe
Woodruff, Robert A.
Belikov, Ruslan
TI SIMULTANEOUS EXOPLANET CHARACTERIZATION AND DEEP WIDE-FIELD IMAGING WITH
A DIFFRACTIVE PUPIL TELESCOPE
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE astrometry; planets and satellites: detection; techniques: high angular
resolution; telescopes
ID PRECISION ASTROMETRY; RADIAL-VELOCITY; PHOTOMETRY; PLANETS; SYSTEMS
AB High-precision astrometry can identify exoplanets and measure their orbits and masses while coronagraphic imaging enables detailed characterization of their physical properties and atmospheric compositions through spectroscopy. In a previous paper, we showed that a diffractive pupil telescope (DPT) in space can enable sub-mu as accuracy astrometric measurements from wide-field images by creating faint but sharp diffraction spikes around the bright target star. The DPT allows simultaneous astrometric measurement and coronagraphic imaging, and we discuss and quantify in this paper the scientific benefits of this combination for exoplanet science investigations: identification of exoplanets with increased sensitivity and robustness, and ability to measure planetary masses to high accuracy. We show how using both measurements to identify planets and measure their masses offers greater sensitivity and provides more reliable measurements than possible with separate missions, and therefore results in a large gain in mission efficiency. The combined measurements reliably identify potentially habitable planets in multiple systems with a few observations, while astrometry or imaging alone would require many measurements over a long time baseline. In addition, the combined measurement allows direct determination of stellar masses to percent-level accuracy, using planets as test particles. We also show that the DPT maintains the full sensitivity of the telescope for deep wide-field imaging, and is therefore compatible with simultaneous scientific observations unrelated to exoplanets. We conclude that astrometry, coronagraphy, and deep wide-field imaging can be performed simultaneously on a single telescope without significant negative impact on the performance of any of the three techniques.
C1 [Guyon, Olivier; Eisner, Josh A.; Angel, Roger; Woolf, Neville J.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA.
[Guyon, Olivier; Martinache, Frantz] Natl Inst Nat Sci, Natl Astron Observ Japan, Subaru Telescope, Hilo, HI 96720 USA.
[Bendek, Eduardo A.; Milster, Thomas D.] Univ Arizona, Coll Opt Sci, Tucson, AZ 85721 USA.
[Ammons, S. Mark] Lawrence Livermore Natl Lab, Phys Div L210, Livermore, CA 94550 USA.
[Shao, Michael; Shaklan, Stuart; Levine, Marie; Nemati, Bijan] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Pitman, Joe] Explorat Sci, Pine, CO 80470 USA.
[Woodruff, Robert A.] Lockheed Martin, Boulder, CO 80304 USA.
[Belikov, Ruslan] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
RP Guyon, O (reprint author), Univ Arizona, Steward Observ, Tucson, AZ 85721 USA.
EM guyon@naoj.org
FU NASA Astronomy and Physics Research and Analysis (APRA) program; State
of Arizona Technology Research Initiative Fund (TRIF); NASA through
Hubble Fellowship grant by the Space Telescope Science Institute
[HST-HF-51250.01-A]; NASA [NAS 5-26555]
FX This work is funded by the NASA Astronomy and Physics Research and
Analysis (APRA) program and the State of Arizona Technology Research
Initiative Fund (TRIF). Support for this work was also provided by NASA
through Hubble Fellowship grant HST-HF-51250.01-A awarded to S. Mark
Ammons by the Space Telescope Science Institute, which is operated by
the Association of Universities for Research in Astronomy, Inc., for
NASA, under contract NAS 5-26555.
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD APR 10
PY 2013
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WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 117IT
UT WOS:000316947500011
ER
PT J
AU Izidoro, A
Torres, KD
Winter, OC
Haghighipour, N
AF Izidoro, A.
de Souza Torres, K.
Winter, O. C.
Haghighipour, N.
TI A COMPOUND MODEL FOR THE ORIGIN OF EARTH'S WATER
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE astrobiology; Earth; planets and satellites: composition; planets and
satellites: formation
ID TERRESTRIAL PLANET FORMATION; INNER SOLAR-SYSTEM; HIGH-RESOLUTION
SIMULATIONS; GIANT PLANETS; DEUTERIUM ENRICHMENT; PROTOPLANETARY DISKS;
DEUTERATED WATER; HABITABLE PLANET; FORMING REGION; UPPER-MANTLE
AB One of the most important subjects of debate in the formation of the solar system is the origin of Earth's water. Comets have long been considered as the most likely source of the delivery of water to Earth. However, elemental and isotopic arguments suggest a very small contribution from these objects. Other sources have also been proposed, among which local adsorption of water vapor onto dust grains in the primordial nebula and delivery through planetesimals and planetary embryos have become more prominent. However, no sole source of water provides a satisfactory explanation for Earth's water as a whole. In view of that, using numerical simulations, we have developed a compound model incorporating both the principal endogenous and exogenous theories, and investigating their implications for terrestrial planet formation and water delivery. Comets are also considered in the final analysis, as it is likely that at least some of Earth's water has cometary origin. We analyze our results comparing two different water distribution models, and complement our study using the D/H ratio, finding possible relative contributions from each source and focusing on planets formed in the habitable zone. We find that the compound model plays an important role by showing greater advantage in the amount and time of water delivery in Earth-like planets.
C1 [Izidoro, A.; Winter, O. C.] Univ Estadual Paulista, UNESP, Grp Dinam Orbital & Planetol, BR-12516410 Sao Paulo, Brazil.
[Haghighipour, N.] Univ Hawaii Manoa, Inst Astron, Honolulu, HI 96822 USA.
[Haghighipour, N.] Univ Hawaii Manoa, NASA Astrobiol Inst, Honolulu, HI 96822 USA.
RP Izidoro, A (reprint author), Univ Estadual Paulista, UNESP, Grp Dinam Orbital & Planetol, BR-12516410 Sao Paulo, Brazil.
EM ocwinter@pq.cnpq.br
FU CAPES (Coordenacao de Aperfeicoamento de Pessoal de Nivel Superior);
CNPq (Conselho Nacional de Desenvolvimento Cientifico e Tecnologico);
FAPESP (Fundacao de Amparo a Pesquisa do Estado de Sao Paulo); NASA
Astrobiology Institute at the Institute for Astronomy, University of
Hawaii [NNA09DA77A]; NASA EXOB grant [NNX09AN05G]
FX We thank the anonymous referee for constructive comments that greatly
improved our manuscript. This work was funded by CAPES (Coordenacao de
Aperfeicoamento de Pessoal de Nivel Superior), CNPq (Conselho Nacional
de Desenvolvimento Cientifico e Tecnologico), and FAPESP (Fundacao de
Amparo a Pesquisa do Estado de Sao Paulo). N.H. acknowledges support
from the NASA Astrobiology Institute under Cooperative Agreement
NNA09DA77A at the Institute for Astronomy, University of Hawaii, and
NASA EXOB grant NNX09AN05G.
NR 81
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD APR 10
PY 2013
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DI 10.1088/0004-637X/767/1/54
PG 20
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 117IT
UT WOS:000316947500054
ER
PT J
AU Karoff, C
Campante, TL
Ballot, J
Kallinger, T
Gruberbauer, M
Garcia, RA
Caldwell, DA
Christiansen, JL
Kinemuchi, K
AF Karoff, C.
Campante, T. L.
Ballot, J.
Kallinger, T.
Gruberbauer, M.
Garcia, R. A.
Caldwell, D. A.
Christiansen, J. L.
Kinemuchi, K.
TI OBSERVATIONS OF INTENSITY FLUCTUATIONS ATTRIBUTED TO GRANULATION AND
FACULAE ON SUN-LIKE STARS FROM THE KEPLER MISSION
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE stars: activity; stars: individual (KIC 6603624, KIC 6933899, KIC
11244118); stars: oscillations; stars: solar-type
ID SOLAR-TYPE STARS; STELLAR OSCILLATIONS; GLOBAL OSCILLATIONS;
MAIN-SEQUENCE; RED GIANTS; P-MODES; FREQUENCY; SPECTRUM;
ASTEROSEISMOLOGY; PERIODICITIES
AB Sun-like stars show intensity fluctuations on a number of timescales due to various physical phenomena on their surfaces. These phenomena can convincingly be studied in the frequency spectra of these stars-while the strongest signatures usually originate from spots, granulation, and p-mode oscillations, it has also been suggested that the frequency spectrum of the Sun contains a signature of faculae. We have analyzed three stars observed for 13 months in short cadence (58.84 s sampling) by the Kepler mission. The frequency spectra of all three stars, as for the Sun, contain signatures that we can attribute to granulation, faculae, and p-mode oscillations. The temporal variability of the signatures attributed to granulation, faculae, and p-mode oscillations was analyzed and the analysis indicates a periodic variability in the granulation and faculae signatures-comparable to what is seen in the Sun.
C1 [Karoff, C.] Aarhus Univ, Dept Phys & Astron, Stellar Astrophys Ctr, DK-8000 Aarhus C, Denmark.
[Campante, T. L.] Univ Porto, Ctr Astrofis, P-4150762 Oporto, Portugal.
[Campante, T. L.] Univ Porto, Fac Ciencias, P-4150762 Oporto, Portugal.
[Campante, T. L.] Univ Birmingham, Sch Phys & Astron, Birmingham B15 2TT, W Midlands, England.
[Ballot, J.] CNRS, Inst Rech Astrophys & Planetol, F-31400 Toulouse, France.
[Ballot, J.] Univ Toulouse, UPS OMP, IRAP, Toulouse, France.
[Kallinger, T.] Katholieke Univ Leuven, Inst Sterrenkunde, B-3001 Louvain, Belgium.
[Kallinger, T.] Univ Vienna, Inst Astron, A-1180 Vienna, Austria.
[Gruberbauer, M.] St Marys Univ, Dept Phys & Astron, Inst Computat Astrophys, Halifax, NS B3H 3C3, Canada.
[Garcia, R. A.] Univ Paris Diderot, IRFU, Ctr Saclay, Lab AIM,CEA,DSM,CNRS,SAp, F-91191 Gif Sur Yvette, France.
[Caldwell, D. A.; Christiansen, J. L.] NASA, Ames Res Ctr, SETI Inst, Moffett Field, CA 94035 USA.
[Kinemuchi, K.] NASA, Ames Res Ctr, Bay Area Environm Res Inst, Moffett Field, CA 94035 USA.
RP Karoff, C (reprint author), Aarhus Univ, Dept Phys & Astron, Stellar Astrophys Ctr, Ny Munkegade 120, DK-8000 Aarhus C, Denmark.
EM karoff@phys.au.dk
RI Caldwell, Douglas/L-7911-2014; Karoff, Christoffer/L-1007-2013;
OI Caldwell, Douglas/0000-0003-1963-9616; Karoff,
Christoffer/0000-0003-2009-7965; Kallinger, Thomas/0000-0003-3627-2561;
Garcia, Rafael/0000-0002-8854-3776
FU NASAs Science Mission Directorate; Carlsberg foundation; FCT/MCTES,
Portugal; UK Science and Technology Facilities Council (STFC);
FWO-Flanders [O6260 - G.0728.11]; Danish National Research Foundation
[DNRF106]; ASTERISK project (ASTERoseismic Investigations with SONG and
Kepler); European Research Council [267864]; [PTDC/CTE-AST/098754/2008]
FX We thank the referee for thoughtful comments, which significantly
improved the paper. Funding for this Discovery mission is provided by
NASAs Science Mission Directorate. The authors wish to thank the entire
Kepler team, without whom these results would not be possible. C. K.
acknowledged support from the Carlsberg foundation. T. L. C.
acknowledges financial support from project PTDC/CTE-AST/098754/2008
funded by FCT/MCTES, Portugal. T. L. C. also acknowledges the support of
the UK Science and Technology Facilities Council (STFC). T. K. is
supported by the FWO-Flanders under project O6260 - G.0728.11. Funding
for the Stellar Astrophysics Centre is provided by The Danish National
Research Foundation (grant agreement No.: DNRF106). The research is
supported by the ASTERISK project (ASTERoseismic Investigations with
SONG and Kepler) funded by the European Research Council (grant
agreement No.: 267864).
NR 58
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD APR 10
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SC Astronomy & Astrophysics
GA 117IT
UT WOS:000316947500034
ER
PT J
AU Kataria, T
Showman, AP
Lewis, NK
Fortney, JJ
Marley, MS
Freedman, RS
AF Kataria, T.
Showman, A. P.
Lewis, N. K.
Fortney, J. J.
Marley, M. S.
Freedman, R. S.
TI THREE-DIMENSIONAL ATMOSPHERIC CIRCULATION OF HOT JUPITERS ON HIGHLY
ECCENTRIC ORBITS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE atmospheric effects; methods: numerical; planets and satellites:
atmospheres; planets and satellites: general
ID TIDALLY LOCKED EXOPLANETS; HD 189733B; EXTRASOLAR PLANET; HYDRODYNAMIC
SIMULATIONS; RADIATIVE-TRANSFER; EMISSION-SPECTRUM; GIANT PLANETS;
MODEL; DYNAMICS; 209458B
AB Of the over 800 exoplanets detected to date, over half are on non-circular orbits, with eccentricities as high as 0.93. Such orbits lead to time-variable stellar heating, which has major implications for the planet's atmospheric dynamical regime. However, little is known about the fundamental dynamical regime of such planetary atmospheres, and how it may influence the observations of these planets. Therefore, we present a systematic study of hot Jupiters on highly eccentric orbits using the SPARC/MITgcm, a model which couples a three-dimensional general circulation model (the MITgcm) with a plane-parallel, two-stream, non-gray radiative transfer model. In our study, we vary the eccentricity and orbit-average stellar flux over a wide range. We demonstrate that the eccentric hot Jupiter regime is qualitatively similar to that of planets on circular orbits; the planets possess a superrotating equatorial jet and exhibit large day-night temperature variations. As in Showman & Polvani, we show that the day-night heating variations induce momentum fluxes equatorward to maintain the superrotating jet throughout its orbit. We find that as the eccentricity and/or stellar flux is increased (corresponding to shorter orbital periods), the superrotating jet strengthens and narrows, due to a smaller Rossby deformation radius. For a select number of model integrations, we generate full-orbit light curves and find that the timing of transit and secondary eclipse viewed from Earth with respect to periapse and apoapse can greatly affect what we see in infrared (IR) light curves; the peak in IR flux can lead or lag secondary eclipse depending on the geometry. For those planets that have large temperature differences from dayside to nightside and rapid rotation rates, we find that the light curves can exhibit "ringing" as the planet's hottest region rotates in and out of view from Earth. These results can be used to explain future observations of eccentric transiting exoplanets.
C1 [Kataria, T.; Showman, A. P.; Lewis, N. K.] Univ Arizona, Dept Planetary Sci, Tucson, AZ 85721 USA.
[Kataria, T.; Showman, A. P.; Lewis, N. K.] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA.
[Lewis, N. K.] MIT, Dept Earth Atmospher & Planetary Sci, Cambridge, MA 02139 USA.
[Fortney, J. J.] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA.
[Marley, M. S.; Freedman, R. S.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Freedman, R. S.] SETI Inst, Mountain View, CA 94043 USA.
RP Kataria, T (reprint author), Univ Arizona, Dept Planetary Sci, Tucson, AZ 85721 USA.
EM tkataria@lpl.arizona.edu
RI Marley, Mark/I-4704-2013;
OI Fortney, Jonathan/0000-0002-9843-4354; Marley, Mark/0000-0002-5251-2943
FU NASA Origins and Planetary Atmospheres; NASA High-End Computing (HEC)
Program through the NASA Advanced Supercomputing (NAS) Division at Ames
Research Center
FX This work was supported by NASA Origins and Planetary Atmospheres grants
to APS. T.K. also acknowledges support from the Harriet P. Jenkins
Pre-Doctoral Fellowship Program (JPFP). Resources supporting this work
were provided by the NASA High-End Computing (HEC) Program through the
NASA Advanced Supercomputing (NAS) Division at Ames Research Center. The
authors thank the anonymous referee for their helpful comments and
suggestions.
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
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JI Astrophys. J.
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SC Astronomy & Astrophysics
GA 117IT
UT WOS:000316947500076
ER
PT J
AU Roettenbacher, RM
Monnier, JD
Harmon, RO
Barclay, T
Still, M
AF Roettenbacher, Rachael M.
Monnier, John D.
Harmon, Robert O.
Barclay, Thomas
Still, Martin
TI IMAGING STARSPOT EVOLUTION ON KEPLER TARGET KIC 5110407 USING
LIGHT-CURVE INVERSION
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE stars: activity; stars: imaging; stars: variables: general
ID BINARY II-PEGASI; CLUSTER NGC 6819; DIFFERENTIAL ROTATION; SPACE
TELESCOPE; STELLAR ACTIVITY; SPOT ACTIVITY; ACTIVE LONGITUDES;
SIGMA-GEMINORUM; INPUT CATALOG; MASS STARS
AB The Kepler target KIC 5110407, a K-type star, shows strong quasi-periodic light curve fluctuations likely arising from the formation and decay of spots on the stellar surface rotating with a period of 3.4693 days. Using an established light-curve inversion algorithm, we study the evolution of the surface features based on Kepler space telescope light curves over a period of two years (with a gap of .25 years). At virtually all epochs, we detect at least one large spot group on the surface causing a 1%-10% flux modulation in the Kepler passband. By identifying and tracking spot groups over a range of inferred latitudes, we measured the surface differential rotation to be much smaller than that found for the Sun. We also searched for a correlation between the 17 stellar flares that occurred during our observations and the orientation of the dominant surface spot at the time of each flare. No statistically significant correlation was found except perhaps for the very brightest flares, suggesting that most flares are associated with regions devoid of spots or spots too small to be clearly discerned using our reconstruction technique. While we may see hints of long-term changes in the spot characteristics and flare statistics within our current data set, a longer baseline of observation will be needed to detect the existence of a magnetic cycle in KIC 5110407.
C1 [Roettenbacher, Rachael M.; Monnier, John D.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA.
[Harmon, Robert O.] Ohio Wesleyan Univ, Dept Phys & Astron, Delaware, OH 43015 USA.
[Barclay, Thomas; Still, Martin] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Barclay, Thomas; Still, Martin] Bay Area Environm Res Inst, Sonoma, CA 95476 USA.
RP Roettenbacher, RM (reprint author), Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA.
EM rmroett@umich.edu
FU NASA Science Mission Directorate; NASA Harriett G. Jenkins Pre-doctoral
Fellowship Program; Cycle 4 Kepler Guest Observer Program (NASA)
[NNX13AC17G]
FX We gratefully acknowledge the helpful and constructive comments from our
referee, Klaus Strassmeier. This paper includes data collected by the
Kepler mission. Funding for the Kepler mission is provided by the NASA
Science Mission Directorate. R. M. R. acknowledges support through the
NASA Harriett G. Jenkins Pre-doctoral Fellowship Program. Additional
support for this project was provided through the Cycle 4 Kepler Guest
Observer Program (NASA grant NNX13AC17G).
NR 47
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD APR 10
PY 2013
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IS 1
AR 60
DI 10.1088/0004-637X/767/1/60
PG 17
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 117IT
UT WOS:000316947500060
ER
PT J
AU Sehgal, N
Addison, G
Battaglia, N
Battistelli, ES
Bond, JR
Das, S
Devlin, MJ
Dunkley, J
Dunner, R
Gralla, M
Hajian, A
Halpern, M
Hasselfield, M
Hilton, M
Hincks, AD
Hlozek, R
Hughes, JP
Kosowsky, A
Lin, YT
Louis, T
Marriage, TA
Marsden, D
Menanteau, F
Moodley, K
Niemack, MD
Page, LA
Partridge, B
Reese, ED
Sherwin, BD
Sievers, J
Sifon, C
Spergel, DN
Staggs, ST
Swetz, DS
Switzer, ER
Wollack, E
AF Sehgal, Neelima
Addison, Graeme
Battaglia, Nick
Battistelli, Elia S.
Bond, J. Richard
Das, Sudeep
Devlin, Mark J.
Dunkley, Joanna
Duenner, Rolando
Gralla, Megan
Hajian, Amir
Halpern, Mark
Hasselfield, Matthew
Hilton, Matt
Hincks, Adam D.
Hlozek, Renee
Hughes, John P.
Kosowsky, Arthur
Lin, Yen-Ting
Louis, Thibaut
Marriage, Tobias A.
Marsden, Danica
Menanteau, Felipe
Moodley, Kavilan
Niemack, Michael D.
Page, Lyman A.
Partridge, Bruce
Reese, Erik D.
Sherwin, Blake D.
Sievers, Jon
Sifon, Cristobal
Spergel, David N.
Staggs, Suzanne T.
Swetz, Daniel S.
Switzer, Eric R.
Wollack, Ed
TI THE ATACAMA COSMOLOGY TELESCOPE: RELATION BETWEEN GALAXY CLUSTER OPTICAL
RICHNESS AND SUNYAEV-ZEL'DOVICH EFFECT
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE cosmic background radiation; galaxies: clusters: general; galaxies:
clusters: intracluster medium
ID SOUTH-POLE TELESCOPE; DIGITAL SKY SURVEY; BACKGROUND POWER SPECTRUM;
SCALING RELATIONS; MAXBCG CLUSTERS; RADIO-SOURCES; 148 GHZ; CONSTRAINTS;
CATALOG; PLANCK
AB We present the measured Sunyaev-Zel'dovich (SZ) flux from 474 optically selected MaxBCG clusters that fall within the Atacama Cosmology Telescope (ACT) Equatorial survey region. The ACT Equatorial region used in this analysis covers 510 deg(2) and overlaps Stripe 82 of the Sloan Digital Sky Survey. We also present the measured SZ flux stacked on 52 X-ray-selected MCXC clusters that fall within the ACT Equatorial region and an ACT Southern survey region covering 455 deg(2). We find that the measured SZ flux from the X-ray-selected clusters is consistent with expectations. However, we find that the measured SZ flux from the optically selected clusters is both significantly lower than expectations and lower than the recovered SZ flux measured by the Planck satellite. Since we find a lower recovered SZ signal than Planck, we investigate the possibility that there is a significant offset between the optically selected brightest cluster galaxies (BCGs) and the SZ centers, to which ACT is more sensitive due to its finer resolution. Such offsets can arise due to either an intrinsic physical separation between the BCG and the center of the gas concentration or from misidentification of the cluster BCG. We find that the entire discrepancy for both ACT and Planck can be explained by assuming that the BCGs are offset from the SZ maxima with a uniform random distribution between 0 and 1.5 Mpc. Such large offsets between gas peaks and BCGs for optically selected cluster samples seem unlikely given that we find the physical separation between BCGs and X-ray peaks for an X-ray-selected subsample of MaxBCG clusters to have a much narrower distribution that peaks within 0.2 Mpc. It is possible that other effects are lowering the ACT and Planck signals by the same amount, with offsets between BCGs and SZ peaks explaining the remaining difference between ACT and Planck measurements. Several effects that can lower the SZ signal equally for both ACT and Planck, but not explain the difference in measured signals, include a larger percentage of false detections in the MaxBCG sample, a lower normalization of the mass-richness relation, radio or infrared galaxy contamination of the SZ flux, and a low intrinsic SZ signal. In the latter two cases, the effects would need to be preferentially more significant in the optically selected MaxBCG sample than in the MCXC X-ray sample.
C1 [Sehgal, Neelima; Hlozek, Renee; Spergel, David N.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA.
[Addison, Graeme; Dunkley, Joanna; Louis, Thibaut] Univ Oxford, Dept Astrophys, Oxford OX1 3RH, England.
[Battaglia, Nick] Carnegie Mellon Univ, Dept Phys, Pittsburgh, PA 15213 USA.
[Battistelli, Elia S.] Univ Roma La Sapienza, Dept Phys, I-00185 Rome, Italy.
[Battistelli, Elia S.; Halpern, Mark; Hasselfield, Matthew] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z4, Canada.
[Bond, J. Richard; Hajian, Amir; Hincks, Adam D.; Sievers, Jon; Switzer, Eric R.] Univ Toronto, Canadian Inst Theoret Astrophys, Toronto, ON M5S 3H8, Canada.
[Das, Sudeep] Univ Calif Berkeley, Berkeley Ctr Cosmol Phys, LBL, Berkeley, CA 94720 USA.
[Das, Sudeep] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA.
[Devlin, Mark J.; Reese, Erik D.] Univ Penn, Dept Phys & Astron, Philadelphia, PA 19104 USA.
[Duenner, Rolando; Sifon, Cristobal] Pontificia Univ Catolica Chile, Dept Astron & Astrofis, Fac Fis, Santiago 22, Chile.
[Gralla, Megan; Marriage, Tobias A.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA.
[Hilton, Matt] Univ Nottingham, Ctr Astron & Particle Theory, Sch Phys & Astron, Nottingham NG7 2RD, England.
[Hincks, Adam D.; Page, Lyman A.; Sherwin, Blake D.; Staggs, Suzanne T.] Princeton Univ, Joseph Henry Labs Phys, Princeton, NJ 08544 USA.
[Hughes, John P.; Menanteau, Felipe] Rutgers State Univ, Dept Phys & Astron, Piscataway, NJ 08854 USA.
[Kosowsky, Arthur] Univ Pittsburgh, Dept Phys & Astron, Pittsburgh, PA 15260 USA.
[Lin, Yen-Ting] Acad Sinica, Inst Astron & Astrophys, Taipei 115, Taiwan.
[Lin, Yen-Ting] Univ Tokyo, Inst Phys & Math Universe, Kashiwa, Chiba 2778568, Japan.
[Marsden, Danica] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA.
[Moodley, Kavilan] Univ KwaZulu Natal, Astrophys & Cosmol Res Unit, Sch Math Sci, ZA-4041 Durban, South Africa.
[Niemack, Michael D.; Swetz, Daniel S.] NIST, Quantum Devices Grp, Boulder, CO 80305 USA.
[Partridge, Bruce] Haverford Coll, Dept Phys & Astron, Haverford, PA 19041 USA.
[Wollack, Ed] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Sehgal, N (reprint author), Princeton Univ, Dept Astrophys Sci, Peyton Hall, Princeton, NJ 08544 USA.
RI Spergel, David/A-4410-2011; Hilton, Matthew James/N-5860-2013; Wollack,
Edward/D-4467-2012;
OI Wollack, Edward/0000-0002-7567-4451; Menanteau,
Felipe/0000-0002-1372-2534; Sievers, Jonathan/0000-0001-6903-5074;
Sifon, Cristobal/0000-0002-8149-1352
FU U.S. National Science Foundation [AST-0408698, PHY-0355328, AST-0707731,
PIRE-0507768, OISE-0530095]; Princeton University; University of
Pennsylvania; Canada Foundation for Innovation (CFI); Compute Canada;
Government of Ontario; Ontario Research Fund-Research Excellence;
University of Toronto; National Science Foundation [1102762, 1066293];
U.S. Department of Energy [DE-AC3-76SF00515]
FX This work was supported by the U.S. National Science Foundation through
awards AST-0408698 for the ACT project, and PHY-0355328, AST-0707731,
and PIRE-0507768 (award number OISE-0530095). The PIRE program made
possible exchanges between Chile, South Africa, Spain, and the U. S.
that enabled this research program. Funding was also provided by
Princeton University, the University of Pennsylvania, and a Canada
Foundation for Innovation (CFI) award to UBC. Computations were
performed on the GPC supercomputer at the SciNet HPC Consortium. SciNet
is funded by the Canada Foundation for Innovation under the auspices of
Compute Canada; the Government of Ontario; Ontario Research
Fund-Research Excellence; and the University of Toronto. ACT is on the
Chajnantor Science preserve, which was made possible by the Chilean
Comision Nacional de Investigacion Cientifica y Tecnologica (CONICYT).
N.S. is supported by the National Science Foundation under Award No.
1102762. During the completion of this work, N.S. was also supported by
the U.S. Department of Energy contract to SLAC No. DE-AC3-76SF00515 and
in part by the National Science Foundation under grant No. 1066293 and
the hospitality of the Aspen Center for Physics. The data will be made
public through LAMBDA (http://lambda.gsfc.nasa.gov/) and the ACT Web
site (http://www.physics.princeton.edu/act/).
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD APR 10
PY 2013
VL 767
IS 1
AR 38
DI 10.1088/0004-637X/767/1/38
PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 117IT
UT WOS:000316947500038
ER
PT J
AU Trott, CM
Tingay, SJ
Wayth, RB
Thompson, DR
Deller, AT
Brisken, WF
Wagstaff, KL
Majid, WA
Burke-Spolaor, S
Macquart, JPR
Palaniswamy, D
AF Trott, Cathryn M.
Tingay, Steven J.
Wayth, Randall B.
Thompson, David R.
Deller, Adam T.
Brisken, Walter F.
Wagstaff, Kiri L.
Majid, Walid A.
Burke-Spolaor, Sarah
Macquart, Jean-Pierre R.
Palaniswamy, Divya
TI A FRAMEWORK FOR INTERPRETING FAST RADIO TRANSIENTS SEARCH EXPERIMENTS:
APPLICATION TO THE V-FASTR EXPERIMENT
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE instrumentation: detectors; methods: data analysis; methods:
observational; radio continuum: general; surveys
ID BASE-LINE ARRAY; PULSAR SURVEY
AB We define a framework for determining constraints on the detection rate of fast transient events from a population of underlying sources, with a view to incorporate beam shape, frequency effects, scattering effects, and detection efficiency into the metric. We then demonstrate a method for combining independent data sets into a single event rate constraint diagram, using a probabilistic approach to the limits on parameter space. We apply this new framework to present the latest results from the V-FASTR experiment, a commensal fast transients search using the Very Long Baseline Array (VLBA). In the 20 cm band, V-FASTR now has the ability to probe the regions of parameter space of importance for the observed Lorimer and Keane fast radio transient candidates by combining the information from observations with differing bandwidths, and properly accounting for the source dispersion measure, VLBA antenna beam shape, experiment time sampling, and stochastic nature of events. We then apply the framework to combine the results of the V-FASTR and Allen Telescope Array Fly's Eye experiments, demonstrating their complementarity. Expectations for fast transients experiments for the SKA Phase I dish array are then computed, and the impact of large differential bandwidths is discussed.
C1 [Trott, Cathryn M.; Tingay, Steven J.; Wayth, Randall B.; Macquart, Jean-Pierre R.; Palaniswamy, Divya] Curtin Univ Technol, Int Ctr Radio Astron Res, Perth, WA 6845, Australia.
[Thompson, David R.; Wagstaff, Kiri L.; Majid, Walid A.; Burke-Spolaor, Sarah] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Deller, Adam T.] ASTRON, NL-7991 PD Dwingeloo, Netherlands.
[Brisken, Walter F.] NRAO, Socorro, NM 87801 USA.
EM cathryn.trott@curtin.edu.au
RI Trott, Cathryn/B-5325-2013; Wayth, Randall/B-2444-2013;
OI Trott, Cathryn/0000-0001-6324-1766; Wayth, Randall/0000-0002-6995-4131;
Deller, Adam/0000-0001-9434-3837; Wagstaff, Kiri/0000-0003-4401-5506
FU State Government of Western Australia; Western Australian Centre of
Excellence in Radio Astronomy Science and Engineering; NRAO Jansky
Fellowship; NWO Veni Fellowship; U.S. National Aeronautics and Space
Administration; [CE110001020]
FX The Centre for All-sky Astrophysics is an Australian Research Council
Centre of Excellence, funded by grant CE110001020. The International
Centre for Radio Astronomy Research (ICRAR) is a Joint Venture between
Curtin University and the University of Western Australia, funded by the
State Government of Western Australia and the Joint Venture partners.
S.J.T. is a Western Australian Premiers Research Fellow. R. B. W. is
supported via the Western Australian Centre of Excellence in Radio
Astronomy Science and Engineering. A. T. D. was supported by an NRAO
Jansky Fellowship and an NWO Veni Fellowship. Part of this research was
carried out at the Jet Propulsion Laboratory, California Institute of
Technology, under contract with the U.S. National Aeronautics and Space
Administration. The National Radio Astronomy Observatory is a facility
of the National Science Foundation operated under cooperative agreement
by Associated Universities, Inc. This research has made use of NASA's
Astrophysics Data System.
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD APR 10
PY 2013
VL 767
IS 1
AR 4
DI 10.1088/0004-637X/767/1/4
PG 9
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 117IT
UT WOS:000316947500004
ER
PT J
AU Weiss, A
De Breuck, C
Marrone, DP
Vieira, JD
Aguirre, JE
Aird, KA
Aravena, M
Ashby, MLN
Bayliss, M
Benson, BA
Bethermin, M
Biggs, AD
Bleem, LE
Bock, JJ
Bothwell, M
Bradford, CM
Brodwin, M
Carlstrom, JE
Chang, CL
Chapman, SC
Crawford, TM
Crites, AT
de Haan, T
Dobbs, MA
Downes, TP
Fassnacht, CD
George, EM
Gladders, MD
Gonzalez, AH
Greve, TR
Halverson, NW
Hezaveh, YD
High, FW
Holder, GP
Holzapfel, WL
Hoover, S
Hrubes, JD
Husband, K
Keisler, R
Lee, AT
Leitch, EM
Lueker, M
Luong-Van, D
Malkan, M
McIntyre, V
McMahon, JJ
Mehl, J
Menten, KM
Meyer, SS
Murphy, EJ
Padin, S
Plagge, T
Reichardt, CL
Rest, A
Rosenman, M
Ruel, J
Ruhl, JE
Schaffer, KK
Shirokoff, E
Spilker, JS
Stalder, B
Staniszewski, Z
Stark, AA
Story, K
Vanderlinde, K
Welikala, N
Williamson, R
AF Weiss, A.
De Breuck, C.
Marrone, D. P.
Vieira, J. D.
Aguirre, J. E.
Aird, K. A.
Aravena, M.
Ashby, M. L. N.
Bayliss, M.
Benson, B. A.
Bethermin, M.
Biggs, A. D.
Bleem, L. E.
Bock, J. J.
Bothwell, M.
Bradford, C. M.
Brodwin, M.
Carlstrom, J. E.
Chang, C. L.
Chapman, S. C.
Crawford, T. M.
Crites, A. T.
de Haan, T.
Dobbs, M. A.
Downes, T. P.
Fassnacht, C. D.
George, E. M.
Gladders, M. D.
Gonzalez, A. H.
Greve, T. R.
Halverson, N. W.
Hezaveh, Y. D.
High, F. W.
Holder, G. P.
Holzapfel, W. L.
Hoover, S.
Hrubes, J. D.
Husband, K.
Keisler, R.
Lee, A. T.
Leitch, E. M.
Lueker, M.
Luong-Van, D.
Malkan, M.
McIntyre, V.
McMahon, J. J.
Mehl, J.
Menten, K. M.
Meyer, S. S.
Murphy, E. J.
Padin, S.
Plagge, T.
Reichardt, C. L.
Rest, A.
Rosenman, M.
Ruel, J.
Ruhl, J. E.
Schaffer, K. K.
Shirokoff, E.
Spilker, J. S.
Stalder, B.
Staniszewski, Z.
Stark, A. A.
Story, K.
Vanderlinde, K.
Welikala, N.
Williamson, R.
TI ALMA REDSHIFTS OF MILLIMETER-SELECTED GALAXIES FROM THE SPT SURVEY: THE
REDSHIFT DISTRIBUTION OF DUSTY STAR-FORMING GALAXIES
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE cosmology: observations; early universe; galaxies: evolution; galaxies:
high-redshift; ISM: molecules
ID HUBBLE-DEEP-FIELD; SOUTH-POLE TELESCOPE; SCUBA SUPER-MAP; DEGREE
EXTRAGALACTIC SURVEY; SUBMILLIMETER GALAXIES; MOLECULAR GAS; FORMATION
HISTORY; NUMBER COUNTS; HERSCHEL ATLAS; LABOCA SURVEY
AB Using the Atacama Large Millimeter/submillimeter Array, we have conducted a blind redshift survey in the 3 mm atmospheric transmission window for 26 strongly lensed dusty star- forming galaxies (DSFGs) selected with the South Pole Telescope. The sources were selected to have S-1.4mm > 20 mJy and a dust- like spectrum and, to remove low- z sources, not have bright radio (S-843MHz < 6 mJy) or far- infrared counterparts (S100 mu m < 1 Jy, S-60 mu m < 200 mJy). We robustly detect 44 line features in our survey, which we identify as redshifted emission lines of (CO)-C-12, (CO)-C-13, CI, H2O, and H2O+. We find one or more spectral features in 23 sources yielding a similar to 90% detection rate for this survey; in 12 of these sources we detect multiple lines, while in 11 sources we detect only a single line. For the sources with only one detected line, we break the redshift degeneracy with additional spectroscopic observations if available, or infer the most likely line identification based on photometric data. This yields secure redshifts for similar to 70% of the sample. The three sources with no lines detected are tentatively placed in the redshift desert between 1.7< z< 2.0. The resulting mean redshift of our sample is z = 3.5. This finding is in contrast to the redshift distribution of radio- identified DSFGs, which have a significantly lower mean redshift of z = 2.3 and for which only 10%- 15% of the population is expected to be at z> 3. We discuss the effect of gravitational lensing on the redshift distribution and compare our measured redshift distribution to that of models in the literature.
C1 [Weiss, A.; Menten, K. M.] Max Planck Inst Radioastron, D-53121 Bonn, Germany.
[De Breuck, C.; Aravena, M.; Biggs, A. D.] European So Observ, D-85748 Garching, Germany.
[Marrone, D. P.; Bothwell, M.; Spilker, J. S.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA.
[Vieira, J. D.; Bock, J. J.; Downes, T. P.; Lueker, M.; Padin, S.; Shirokoff, E.; Staniszewski, Z.] CALTECH, Pasadena, CA 91125 USA.
[Aguirre, J. E.; Rosenman, M.] Univ Penn, Philadelphia, PA 19104 USA.
[Aird, K. A.; Hrubes, J. D.; Luong-Van, D.] Univ Chicago, Chicago, IL 60637 USA.
[Ashby, M. L. N.; Bayliss, M.; Stalder, B.; Stark, A. A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Bayliss, M.; Ruel, J.] Harvard Univ, Dept Phys, Cambridge, MA 02138 USA.
[Benson, B. A.; Bleem, L. E.; Carlstrom, J. E.; Chang, C. L.; Crawford, T. M.; Crites, A. T.; Gladders, M. D.; High, F. W.; Hoover, S.; Keisler, R.; Leitch, E. M.; McMahon, J. J.; Mehl, J.; Meyer, S. S.; Padin, S.; Plagge, T.; Schaffer, K. K.; Story, K.; Williamson, R.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA.
[Benson, B. A.; Carlstrom, J. E.; Chang, C. L.; Hoover, S.; McMahon, J. J.; Meyer, S. S.] Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA.
[Bethermin, M.] Univ Paris Diderot, CEA Saclay, CNRS, CEA,DSM,Irfu,Lab AIM Paris Saclay, F-91191 Gif Sur Yvette, France.
[Bleem, L. E.; Carlstrom, J. E.; Keisler, R.; Meyer, S. S.; Story, K.] Univ Chicago, Dept Phys, Chicago, IL 60637 USA.
[Bock, J. J.; Bradford, C. M.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Brodwin, M.] Univ Missouri, Dept Phys & Astron, Kansas City, MO 64110 USA.
[Carlstrom, J. E.; Crawford, T. M.; Crites, A. T.; Gladders, M. D.; High, F. W.; Leitch, E. M.; Mehl, J.; Meyer, S. S.; Padin, S.; Plagge, T.; Williamson, R.] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA.
[Carlstrom, J. E.; Chang, C. L.] Argonne Natl Lab, Argonne, IL 60439 USA.
[Chapman, S. C.] Dalhousie Univ, Dept Phys & Atmospher Sci, Halifax, NS B3H 3J5, Canada.
[Chapman, S. C.; Husband, K.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England.
[de Haan, T.; Dobbs, M. A.; Hezaveh, Y. D.; Holder, G. P.; Vanderlinde, K.] McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada.
[Fassnacht, C. D.] Univ Calif Davis, Dept Phys, Davis, CA 95616 USA.
[George, E. M.; Holzapfel, W. L.; Lee, A. T.; Reichardt, C. L.] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA.
[Gonzalez, A. H.] Univ Florida, Dept Astron, Gainesville, FL 32611 USA.
[Greve, T. R.] UCL, Dept Phys & Astron, London WC1E 6BT, England.
[Halverson, N. W.] Univ Colorado, Dept Astrophys & Planetary Sci, Boulder, CO 80309 USA.
[Halverson, N. W.] Univ Colorado, Dept Phys, Boulder, CO 80309 USA.
[Lee, A. T.] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Div Phys, Berkeley, CA 94720 USA.
[Malkan, M.] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA.
[McIntyre, V.] CSIRO, Australia Telescope Natl Facil, Epping, NSW 1710, Australia.
[McMahon, J. J.] Univ Michigan, Dept Phys, Ann Arbor, MI 48109 USA.
[Murphy, E. J.] Observ Carnegie Inst Sci, Pasadena, CA 91101 USA.
[Rest, A.] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
[Ruhl, J. E.; Staniszewski, Z.] Case Western Reserve Univ, Dept Phys, Ctr Educ & Res Cosmol & Astrophys, Cleveland, OH 44106 USA.
[Schaffer, K. K.] Sch Art Inst Chicago, Liberal Arts Dept, Chicago, IL 60603 USA.
[Welikala, N.] Univ Paris 11, Inst Astrophys Spatiale, F-91405 Orsay, France.
[Welikala, N.] CNRS, F-91405 Orsay, France.
RP Weiss, A (reprint author), Max Planck Inst Radioastron, Hugel 69, D-53121 Bonn, Germany.
RI Aravena, Manuel/O-2361-2014; Williamson, Ross/H-1734-2015; Holzapfel,
William/I-4836-2015;
OI Williamson, Ross/0000-0002-6945-2975; Marrone,
Daniel/0000-0002-2367-1080; Aird, Kenneth/0000-0003-1441-9518;
Reichardt, Christian/0000-0003-2226-9169; De Breuck,
Carlos/0000-0002-6637-3315; Bethermin, Matthieu/0000-0002-3915-2015;
Stark, Antony/0000-0002-2718-9996
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD APR 10
PY 2013
VL 767
IS 1
AR 88
DI 10.1088/0004-637X/767/1/88
PG 16
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 117IT
UT WOS:000316947500088
ER
PT J
AU Zhang, YC
Tan, JC
De Buizer, JM
Sandell, G
Beltran, MT
Churchwell, E
McKee, CF
Shuping, R
Staff, JE
Telesco, C
Whitney, B
AF Zhang, Yichen
Tan, Jonathan C.
De Buizer, James M.
Sandell, Goeran
Beltran, Maria T.
Churchwell, Ed
McKee, Christopher F.
Shuping, Ralph
Staff, Jan E.
Telesco, Charles
Whitney, Barbara
TI A MASSIVE PROTOSTAR FORMING BY ORDERED COLLAPSE OF A DENSE, MASSIVE CORE
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE stars: formation
ID STAR-FORMATION; MOLECULAR OUTFLOWS; G35.2-0.74N; G35.20-0.74; CLUSTER;
CLUMPS; VIEW; JET
AB We present 30 and 40 mu m imaging of the massive protostar G35.20-0.74 with SOFIA-FORCAST. The high surface density of the natal core around the protostar leads to high extinction, even at these relatively long wavelengths, causing the observed flux to be dominated by that emerging from the near-facing outflow cavity. However, emission from the far-facing cavity is still clearly detected. We combine these results with fluxes from the near-infrared to mm to construct a spectral energy distribution (SED). For isotropic emission the bolometric luminosity would be 3.3 x 10(4) L-circle dot. We perform radiative transfer modeling of a protostar forming by ordered, symmetric collapse from a massive core bounded by a clump with high-mass surface density, Sigma(cl). To fit the SED requires protostellar masses similar to 20-34 M-circle dot depending on the outflow cavity opening angle (35 degrees-50 degrees), and Sigma(cl) similar to 0.4-1 g cm(-2). After accounting for the foreground extinction and the flashlight effect, the true bolometric luminosity is similar to(0.7-2.2) x 10(5) L-circle dot. One of these models also has excellent agreement with the observed intensity profiles along the outflow axis at 10, 18, 31, and 37 mu m. Overall our results support a model of massive star formation involving the relatively ordered, symmetric collapse of a massive, dense core and the launching bipolar outflows that clear low-density cavities. Thus a unified model may apply for the formation of both low- and high-mass stars.
C1 [Zhang, Yichen; Tan, Jonathan C.; Telesco, Charles] Univ Florida, Dept Astron, Gainesville, FL 32611 USA.
[Tan, Jonathan C.] Univ Florida, Dept Phys, Gainesville, FL 32611 USA.
[De Buizer, James M.; Sandell, Goeran; Shuping, Ralph] NASA, SOFIA USRA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Beltran, Maria T.] INAF Osservatorio Astrofis Arcetri, I-50125 Florence, Italy.
[Churchwell, Ed; Whitney, Barbara] Univ Wisconsin, Dept Astron, Madison, WI 53706 USA.
[McKee, Christopher F.] Univ Calif Berkeley, Dept Astron & Astrophys, Berkeley, CA 94720 USA.
[McKee, Christopher F.] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA.
[Staff, Jan E.] Louisiana State Univ, Dept Phys & Astron, Baton Rouge, LA 70803 USA.
RP Zhang, YC (reprint author), Univ Florida, Dept Astron, Gainesville, FL 32611 USA.
EM yc.zhang@astro.ufl.edu
OI Beltran Sorolla, Maria Teresa/0000-0003-3315-5626
FU NASA [NAS2-97001, NNX09AK31G]; Deutsches SOFIA Institut (DSI) under DLR
[50 OK 0901]; University of Florida; NSF CAREER [AST-0645412];
NASA/USRA; NSF [AST-0908553, AST-1211729]
FX This work is based on observations made with the NASA/DLR Stratospheric
Observatory for Infrared Astronomy (SOFIA). SOFIA is jointly operated by
the Universities Space Research Association, Inc. (USRA), under NASA
contract NAS2-97001, and the Deutsches SOFIA Institut (DSI) under DLR
contract 50 OK 0901 to the University of Stuttgart. Y.Z. acknowledges
support from a Graduate School Fellowship from the University of
Florida. J.C.T. acknowledges support from NSF CAREER grant AST-0645412
and NASA/USRA grant in support of SOFIA Basic Science observations. C.
F. M. acknowledges support from NSF grants AST-0908553 and AST-1211729
and NASA grant NNX09AK31G.
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PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD APR 10
PY 2013
VL 767
IS 1
AR 58
DI 10.1088/0004-637X/767/1/58
PG 6
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 117IT
UT WOS:000316947500058
ER
PT J
AU Kopparapu, RK
AF Kopparapu, Ravi Kumar
TI A REVISED ESTIMATE OF THE OCCURRENCE RATE OF TERRESTRIAL PLANETS IN THE
HABITABLE ZONES AROUND KEPLER M-DWARFS
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE planets and satellites: atmospheres
ID M-CIRCLE-PLUS; SUPER-EARTH; STARS; CANDIDATES; SYSTEM; EVOLUTION;
DATABASE; SEARCH; MODELS; MARS
AB Because of their large numbers, low-mass stars may be the most abundant planet hosts in our Galaxy. Furthermore, terrestrial planets in the habitable zones (HZs) around M-dwarfs can potentially be characterized in the near future and hence may be the first such planets to be studied. Recently, Dressing & Charbonneau used Kepler data and calculated the frequency of terrestrial planets in the HZ of cool stars to be 0.15(-0.06)(+0.13) per star for Earth-size planets (0.5-1.4 R-circle plus). However, this estimate was derived using the Kasting et al. HZ limits, which were not valid for stars with effective temperatures lower than 3700 K. Here we update their result using new HZ limits from Kopparapu et al. for stars with effective temperatures between 2600 K and 7200 K, which includes the cool M stars in the Kepler target list. The new HZ boundaries increase the number of planet candidates in the HZ. Assuming Earth- size planets as 0.5- 1.4 R-circle plus, when we reanalyze their results, we obtain a terrestrial planet frequency of 0.48(- 0.24)(+0.12) and 0.53(-0.17)(+0.08) planets per M-dwarf star for conservative and optimistic limits of the HZ boundaries, respectively. Assuming Earth- size planets as 0.5-2 R-circle plus, the frequency increases to 0.51(-0.20)(+0.10) per star for the conservative estimate and to 0.61(-0.15)(+0.07) per star for the optimistic estimate. Within uncertainties, our optimistic estimates are in agreement with a similar optimistic estimate from the radial velocity survey of M-dwarfs (0.41(-0.13)(+0.54)). So, the potential for finding Earth- like planets around M stars may be higher than previously reported.
C1 [Kopparapu, Ravi Kumar] Penn State Univ, Dept Geosci, University Pk, PA 16802 USA.
[Kopparapu, Ravi Kumar] Penn State Astrobiol Res Ctr, University Pk, PA 16802 USA.
[Kopparapu, Ravi Kumar] Penn State Univ, Ctr Exoplanets & Habitable Worlds, University Pk, PA 16802 USA.
RP Kopparapu, RK (reprint author), NASA, Astrobiol Inst Virtual Planetary Lab, Washington, DC USA.
FU NASA Astrobiology Institute's Virtual Planetary Laboratory lead team;
NASA [NNH05ZDA001C]; Penn State Astrobiology Research Center
FX The author is grateful to Courtney Dressing for discussions leading to
this paper. The author thanks James Kasting, Steinn Sigurdsson, Eric
Feigelson, Suvrath Mahadevan, Jason Wright, Chester Harman, and Ramses
Ramirez for their valuable input and the anonymous referee whose
comments improved the manuscript. R.K. gratefully acknowledges funding
from NASA Astrobiology Institute's Virtual Planetary Laboratory lead
team, supported by NASA under cooperative agreement NNH05ZDA001C, and
the Penn State Astrobiology Research Center.
NR 31
TC 79
Z9 79
U1 1
U2 22
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 2041-8205
J9 ASTROPHYS J LETT
JI Astrophys. J. Lett.
PD APR 10
PY 2013
VL 767
IS 1
AR L8
DI 10.1088/2041-8205/767/1/L8
PG 5
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 118CB
UT WOS:000316998900008
ER
PT J
AU Nersisyan, SR
Tabiryan, NV
Mawet, D
Serabyn, E
AF Nersisyan, Sarik R.
Tabiryan, Nelson V.
Mawet, Dimitri
Serabyn, Eugene
TI Improving vector vortex waveplates for high-contrast coronagraphy
SO OPTICS EXPRESS
LA English
DT Article
AB Vector vortex waveplates (VVWs) open the door to new techniques in stellar coronagraphy and optical communications, but the performance of currently available liquid-crystal-polymer-based VVWs tends to be limited by defects in the axial region of the vortex pattern. As described here, several steps allow for a reduction in the size of such axial defects, including the use of photoalignment materials with high photosensitivity and reversible response, and a reduction in exposure energy. Moreover, redistributing the writing beam's intensity from the axial region to its periphery (using a VVW) allows the production of large area VVWs with a small defect area. Finally, using VVWs as linear to axial polarization converters allows producing VVWs of higher topological charge, while also reducing the photoalignment time to a few minutes. These steps have allowed the fabrication of VVWs with topological charges of 1 and 2 with central defect sizes below 3 mu m. (C)2013 Optical Society of America
C1 [Nersisyan, Sarik R.; Tabiryan, Nelson V.] BEAM Engn Adv Measurements Co, Winter Pk, FL 32789 USA.
[Mawet, Dimitri] European So Observ, Santiago 19, Chile.
[Serabyn, Eugene] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Nersisyan, SR (reprint author), BEAM Engn Adv Measurements Co, 809 S Orlando Ave,Suite 1, Winter Pk, FL 32789 USA.
EM nelson@beamco.com
FU NASA SBIR Program [NNX11CF39P]
FX The study was supported by NASA SBIR Program (Contract no. NNX11CF39P).
Part of this work was carried out at the Jet Propulsion Laboratory,
California Institute of Technology, under contract with NASA.
NR 15
TC 21
Z9 21
U1 2
U2 21
PU OPTICAL SOC AMER
PI WASHINGTON
PA 2010 MASSACHUSETTS AVE NW, WASHINGTON, DC 20036 USA
SN 1094-4087
J9 OPT EXPRESS
JI Opt. Express
PD APR 8
PY 2013
VL 21
IS 7
BP 8205
EP 8213
DI 10.1364/OE.21.008205
PG 9
WC Optics
SC Optics
GA 126YN
UT WOS:000317659300036
PM 23571910
ER
PT J
AU Kaul, AB
Coles, JB
Eastwood, M
Green, RO
Bandaru, PR
AF Kaul, Anupama B.
Coles, James B.
Eastwood, Michael
Green, Robert O.
Bandaru, Prabhakar R.
TI Ultra-High Optical Absorption Efficiency from the Ultraviolet to the
Infrared Using Multi-Walled Carbon Nanotube Ensembles
SO SMALL
LA English
DT Article
DE optical absorbers; nanoabsorbers; nanomaterials; carbon nanotubes
ID SILICON NANOWIRE; ABSORBER; ARRAYS; DEPOSITION; CATALYST; DENSITY;
GROWTH
AB The optical absorption efficiencies of vertically aligned multi-walled (MW)-carbon nanotube (CNT) ensembles are characterized in the 3507000 nm wavelength range where CNT site densities > 1 x 1011/cm2 are achieved directly on metallic substrates. The site density directly impacts the optical absorption characteristics, and while high-density arrays of CNTs on electrically insulating and non-metallic substrates have been commonly reported, achieving high site-densities on metals has been challenging and remains an area of active research. These absorber ensembles are ultra-thin (<10 m) and yet they still exhibit a reflectance as low as approximate to 0.02%, which is 100 times lower than the reference; these characteristics make them potentially attractive for high-sensitivity and high-speed thermal detectors. In addition, the use of a plasma-enhanced chemical vapor deposition process for the synthesis of the absorbers increases the portfolio of materials that can be integrated with such absorbers due to the potential for reduced synthesis temperatures. The remarkable ruggedness of the absorbers is also demonstrated as they are exposed to high temperatures in an oxidizing ambient environment, making them well-suited for extreme thermal environments encountered in the field, potentially for solar cell applications. Finally, a phenomenological model enables the determinatiom of the extinction coefficients in these nanostructures and the results compare well with experiment.
C1 [Kaul, Anupama B.; Coles, James B.; Eastwood, Michael; Green, Robert O.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Bandaru, Prabhakar R.] Univ Calif San Diego, Jacobs Sch Engn, La Jolla, CA 92093 USA.
RP Kaul, AB (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM Anupama.B.Kaul@jpl.nasa.gov
FU internal Research and Technology Development (RTD) program [01STCR,
R.10.021.067]; National Science Foundation
FX We thank K. Megerian, M. Anderson, and R. Kowalczyk for technical
assistance and T. Pagano, P. Goldsmith, J. Hyon, M. Foote, and W. Holmes
for useful discussions. This research was carried out at the Jet
Propulsion Laboratory, California Institute of Technology, under a
contract with the National Aeronautics and Space Administration and was
funded through the internal Research and Technology Development (R&TD)
program (01STCR, R.10.021.067). ABK also acknowledges support for this
work through the National Science Foundation's IR/D program.
NR 27
TC 13
Z9 13
U1 7
U2 70
PU WILEY-V C H VERLAG GMBH
PI WEINHEIM
PA BOSCHSTRASSE 12, D-69469 WEINHEIM, GERMANY
SN 1613-6810
J9 SMALL
JI Small
PD APR 8
PY 2013
VL 9
IS 7
BP 1058
EP 1065
DI 10.1002/smll.201202232
PG 8
WC Chemistry, Multidisciplinary; Chemistry, Physical; Nanoscience &
Nanotechnology; Materials Science, Multidisciplinary; Physics, Applied;
Physics, Condensed Matter
SC Chemistry; Science & Technology - Other Topics; Materials Science;
Physics
GA 118IT
UT WOS:000317019800016
PM 23233398
ER
PT J
AU Blake, DR
Simpson, IJ
Meinardi, SJ
Andersen, MJS
Bruhwiler, L
AF Blake, Donald R.
Simpson, Isobel J.
Meinardi, Simone J.
Andersen, Mads J. Sulbaek
Bruhwiler, Lori
TI Award Address (ACS Award for Creative Advances in Environmental Science
and Technology sponsored by ACS Division of Environmental Chemistry and
ACS Publications Divisions). Long-term trends in global concentrations
of atmospheric methane and ethane
SO ABSTRACTS OF PAPERS OF THE AMERICAN CHEMICAL SOCIETY
LA English
DT Meeting Abstract
CT 245th National Spring Meeting of the American-Chemical-Society (ACS)
CY APR 07-11, 2013
CL New Orleans, LA
SP Amer Chem Soc
C1 [Blake, Donald R.; Simpson, Isobel J.; Meinardi, Simone J.] Univ Calif Irvine, Irvine, CA 92617 USA.
[Andersen, Mads J. Sulbaek] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Bruhwiler, Lori] NOAA Earth Syst Res Lab ESRL, Boulder, CO 80305 USA.
EM drblake@uci.edu
NR 0
TC 0
Z9 0
U1 0
U2 1
PU AMER CHEMICAL SOC
PI WASHINGTON
PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA
SN 0065-7727
J9 ABSTR PAP AM CHEM S
JI Abstr. Pap. Am. Chem. Soc.
PD APR 7
PY 2013
VL 245
MA 241-ENVR
PG 1
WC Chemistry, Multidisciplinary
SC Chemistry
GA 216SF
UT WOS:000324303600089
ER
PT J
AU Chu, SH
Park, C
Lowther, SE
Gibbons, LJ
Sauti, G
Kang, JH
Thibeault, SA
Fay, CC
Bryant, RG
AF Chu, Sang-Hyon
Park, Cheol
Lowther, Sharon E.
Gibbons, Luke J.
Sauti, Godfrey
Kang, Jin Ho
Thibeault, Sheila A.
Fay, Catharine C.
Bryant, Robert G.
TI Porous polyimide nanocomposite films with high neutron absorption
effectiveness
SO ABSTRACTS OF PAPERS OF THE AMERICAN CHEMICAL SOCIETY
LA English
DT Meeting Abstract
CT 245th National Spring Meeting of the American-Chemical-Society (ACS)
CY APR 07-11, 2013
CL New Orleans, LA
SP Amer Chem Soc
C1 [Chu, Sang-Hyon; Park, Cheol; Gibbons, Luke J.; Sauti, Godfrey; Kang, Jin Ho] Natl Inst Aerosp, Hampton, VA 23666 USA.
[Lowther, Sharon E.; Thibeault, Sheila A.; Fay, Catharine C.; Bryant, Robert G.] NASA Langley Res Ctr, Hampton, VA 23681 USA.
EM sang-hyon.chu-1@nasa.gov
NR 0
TC 0
Z9 0
U1 0
U2 4
PU AMER CHEMICAL SOC
PI WASHINGTON
PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA
SN 0065-7727
J9 ABSTR PAP AM CHEM S
JI Abstr. Pap. Am. Chem. Soc.
PD APR 7
PY 2013
VL 245
MA 488-PMSE
PG 1
WC Chemistry, Multidisciplinary
SC Chemistry
GA 216SF
UT WOS:000324303604437
ER
PT J
AU Guo, HQ
Meador, MAB
Bali, S
McCorkle, L
Guo, J
Hamilton, B
Cakmak, M
AF Guo, Haiquan
Meador, Mary Ann B.
Bali, Sheeba
McCorkle, Linda
Guo, Jiao
Hamilton, Bart
Cakmak, Miko
TI Optimization of properties of cross-linked polyimide aerogels for high
temperature aerospace applications
SO ABSTRACTS OF PAPERS OF THE AMERICAN CHEMICAL SOCIETY
LA English
DT Meeting Abstract
CT 245th National Spring Meeting of the American-Chemical-Society (ACS)
CY APR 07-11, 2013
CL New Orleans, LA
SP Amer Chem Soc
C1 [Guo, Haiquan; McCorkle, Linda] Ohio Aerosp Inst, Cleveland, OH 44142 USA.
[Meador, Mary Ann B.; Bali, Sheeba] NASA Glenn Res Ctr, Cleveland, OH 44135 USA.
[Guo, Jiao; Hamilton, Bart; Cakmak, Miko] Univ Akron, Akron, OH 44325 USA.
EM haiquan.n.guo@nasa.gov
NR 0
TC 0
Z9 1
U1 1
U2 3
PU AMER CHEMICAL SOC
PI WASHINGTON
PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA
SN 0065-7727
J9 ABSTR PAP AM CHEM S
JI Abstr. Pap. Am. Chem. Soc.
PD APR 7
PY 2013
VL 245
MA 358-PMSE
PG 1
WC Chemistry, Multidisciplinary
SC Chemistry
GA 216SF
UT WOS:000324303604306
ER
PT J
AU Li, J
Klankowski, S
Rojeski, R
Cruden, BA
Liu, JW
Wu, J
AF Li, Jun
Klankowski, Steven
Rojeski, Ronald
Cruden, Brett A.
Liu, Jianwei
Wu, Judy
TI High-performance lithium-ion battery anode based on core-shell
heterostructure of silicon-coated vertically aligned carbon nanofibers
SO ABSTRACTS OF PAPERS OF THE AMERICAN CHEMICAL SOCIETY
LA English
DT Meeting Abstract
CT 245th National Spring Meeting of the American-Chemical-Society (ACS)
CY APR 07-11, 2013
CL New Orleans, LA
SP Amer Chem Soc
C1 [Li, Jun; Klankowski, Steven] Kansas State Univ, Dept Chem, Manhattan, KS 66506 USA.
[Rojeski, Ronald] Catalyst Power Technol, Campbell, CA 95008 USA.
[Cruden, Brett A.] NASA Ames Res Ctr, Ctr Nanotechnol, Moffett Field, CA 94035 USA.
[Liu, Jianwei; Wu, Judy] Univ Kansas, Dept Phys & Astron, Lawrence, KS 66045 USA.
EM junli@ksu.edu
NR 0
TC 0
Z9 0
U1 0
U2 8
PU AMER CHEMICAL SOC
PI WASHINGTON
PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA
SN 0065-7727
J9 ABSTR PAP AM CHEM S
JI Abstr. Pap. Am. Chem. Soc.
PD APR 7
PY 2013
VL 245
MA 30-IEC
PG 1
WC Chemistry, Multidisciplinary
SC Chemistry
GA 216SF
UT WOS:000324303600622
ER
PT J
AU Meador, MAB
Miranda, FA
Wright, S
Sandberg, A
Nguyen, BN
Van Keuls, FW
Mueller, CH
Rodriguez, R
AF Meador, Mary Ann B.
Miranda, Felix A.
Wright, Sarah
Sandberg, Anna
Nguyen, Baochau N.
Van Keuls, Frederick W.
Mueller, Carl H.
Rodriguez, Rafael
TI Low dielectric polyimide aerogels as substrates for lightweight patch
antennas
SO ABSTRACTS OF PAPERS OF THE AMERICAN CHEMICAL SOCIETY
LA English
DT Meeting Abstract
CT 245th National Spring Meeting of the American-Chemical-Society (ACS)
CY APR 07-11, 2013
CL New Orleans, LA
SP Amer Chem Soc
C1 [Meador, Mary Ann B.; Miranda, Felix A.; Wright, Sarah; Sandberg, Anna; Van Keuls, Frederick W.; Mueller, Carl H.; Rodriguez, Rafael] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA.
[Nguyen, Baochau N.] Ohio Aerosp Inst, Cleveland, OH 44142 USA.
EM maryann.meador@nasa.gov
NR 0
TC 0
Z9 0
U1 5
U2 6
PU AMER CHEMICAL SOC
PI WASHINGTON
PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA
SN 0065-7727
J9 ABSTR PAP AM CHEM S
JI Abstr. Pap. Am. Chem. Soc.
PD APR 7
PY 2013
VL 245
MA 241-PMSE
PG 1
WC Chemistry, Multidisciplinary
SC Chemistry
GA 216SF
UT WOS:000324303604182
ER
PT J
AU Vance, S
Christensen, L
AF Vance, Steve
Christensen, Lance
TI In situ characterization of naturally occurring methane and ethane at
sites of active serpentinization by tunable diode laser spectroscopy
SO ABSTRACTS OF PAPERS OF THE AMERICAN CHEMICAL SOCIETY
LA English
DT Meeting Abstract
CT 245th National Spring Meeting of the American-Chemical-Society (ACS)
CY APR 07-11, 2013
CL New Orleans, LA
SP Amer Chem Soc
C1 [Vance, Steve; Christensen, Lance] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
EM svance@jpl.nasa.gov
NR 0
TC 0
Z9 0
U1 0
U2 1
PU AMER CHEMICAL SOC
PI WASHINGTON
PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA
SN 0065-7727
J9 ABSTR PAP AM CHEM S
JI Abstr. Pap. Am. Chem. Soc.
PD APR 7
PY 2013
VL 245
MA 93-GEOC
PG 1
WC Chemistry, Multidisciplinary
SC Chemistry
GA 216SF
UT WOS:000324303600534
ER
PT J
AU Wojtecki, RJ
Johnson, JC
Meador, MA
Rowan, SJ
AF Wojtecki, Rudy J.
Johnson, J. Casey
Meador, Michael A.
Rowan, Stuart J.
TI Toward the design and synthesis of mechanically interlocked polymers
SO ABSTRACTS OF PAPERS OF THE AMERICAN CHEMICAL SOCIETY
LA English
DT Meeting Abstract
CT 245th National Spring Meeting of the American-Chemical-Society (ACS)
CY APR 07-11, 2013
CL New Orleans, LA
SP Amer Chem Soc
C1 [Wojtecki, Rudy J.; Johnson, J. Casey; Rowan, Stuart J.] Case Western Reserve Univ, Cleveland, OH 44106 USA.
[Meador, Michael A.] NASA, Glenn Res Ctr, Dept Nanotechnol Res, Cleveland, OH 44135 USA.
EM rjw41@case.edu
NR 0
TC 0
Z9 0
U1 0
U2 0
PU AMER CHEMICAL SOC
PI WASHINGTON
PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA
SN 0065-7727
J9 ABSTR PAP AM CHEM S
JI Abstr. Pap. Am. Chem. Soc.
PD APR 7
PY 2013
VL 245
MA 526-ORGN
PG 1
WC Chemistry, Multidisciplinary
SC Chemistry
GA 216SF
UT WOS:000324303603197
ER
PT J
AU Barzen-Hanson, K
Uz-Zaman, A
Oye, M
Meyyapan, M
Koehne, J
AF Barzen-Hanson, Krista
Uz-Zaman, Asma
Oye, Michael
Meyyapan, Meyya
Koehne, Jessica
TI Growth optimization of monolayer graphene films using chemical vapor
deposition
SO ABSTRACTS OF PAPERS OF THE AMERICAN CHEMICAL SOCIETY
LA English
DT Meeting Abstract
CT 245th National Meeting of the American-Chemical-Society (ACS)
CY APR 07-11, 2013
CL New Orleans, LA
SP Amer Chem Soc
C1 [Barzen-Hanson, Krista] Coll St Benedict, Dept Chem, St Joseph, MN 56374 USA.
[Uz-Zaman, Asma] Univ Calif Santa Cruz, Santa Cruz, CA 95064 USA.
[Oye, Michael; Meyyapan, Meyya; Koehne, Jessica] NASA, Ames Res Ctr, Ctr Nanotechnol, Moffett Field, CA 94035 USA.
EM kabarzenhanson@csbsju.edu
NR 0
TC 0
Z9 0
U1 0
U2 4
PU AMER CHEMICAL SOC
PI WASHINGTON
PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA
SN 0065-7727
J9 ABSTR PAP AM CHEM S
JI Abstr. Pap. Am. Chem. Soc.
PD APR 7
PY 2013
VL 245
MA 844-CHED
PG 1
WC Chemistry, Multidisciplinary
SC Chemistry
GA 210RD
UT WOS:000323851302637
ER
PT J
AU Fortenberry, RC
Huang, XC
Lee, TJ
AF Fortenberry, Ryan C.
Huang, Xinchuan
Lee, Timothy J.
TI Quartic force fields and dipole surfaces for accurate computational
rovibrational reference data for interstellar studies
SO ABSTRACTS OF PAPERS OF THE AMERICAN CHEMICAL SOCIETY
LA English
DT Meeting Abstract
CT 245th National Meeting of the American-Chemical-Society (ACS)
CY APR 07-11, 2013
CL New Orleans, LA
SP Amer Chem Soc
C1 [Fortenberry, Ryan C.; Lee, Timothy J.] NASA, Space Sci & Astrobiol Div, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Huang, Xinchuan] SETI Inst, Mountain View, CA 94043 USA.
EM ryan.c.fortenberry@nasa.gov
RI HUANG, XINCHUAN/A-3266-2013
NR 0
TC 0
Z9 0
U1 0
U2 0
PU AMER CHEMICAL SOC
PI WASHINGTON
PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA
SN 0065-7727
J9 ABSTR PAP AM CHEM S
JI Abstr. Pap. Am. Chem. Soc.
PD APR 7
PY 2013
VL 245
MA 391-COMP
PG 1
WC Chemistry, Multidisciplinary
SC Chemistry
GA 210RD
UT WOS:000323851304396
ER
PT J
AU Holt, B
Jones, CE
Minchew, B
Brekke, C
AF Holt, Benjamin
Jones, Cathleen E.
Minchew, Brent
Brekke, Camilla
TI Deepwater Horizon oil slick characterization with UAVSAR: Continuing
investigations
SO ABSTRACTS OF PAPERS OF THE AMERICAN CHEMICAL SOCIETY
LA English
DT Meeting Abstract
CT 245th National Meeting of the American-Chemical-Society (ACS)
CY APR 07-11, 2013
CL New Orleans, LA
SP Amer Chem Soc
C1 [Holt, Benjamin; Jones, Cathleen E.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Minchew, Brent] CALTECH, Pasadena, CA 91125 USA.
[Brekke, Camilla] Univ Tromso, Tromso, Norway.
EM Benjamin.M.Holt@jpl.nasa.gov
NR 0
TC 0
Z9 0
U1 0
U2 3
PU AMER CHEMICAL SOC
PI WASHINGTON
PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA
SN 0065-7727
J9 ABSTR PAP AM CHEM S
JI Abstr. Pap. Am. Chem. Soc.
PD APR 7
PY 2013
VL 245
MA 223-ANYL
PG 1
WC Chemistry, Multidisciplinary
SC Chemistry
GA 210RD
UT WOS:000323851300440
ER
PT J
AU Rajput, NN
Monk, J
Hung, FR
AF Rajput, Nav N.
Monk, Joshua
Hung, Francisco R.
TI Ionic liquids confined inside model nanoporous carbons: A molecular
simulation study
SO ABSTRACTS OF PAPERS OF THE AMERICAN CHEMICAL SOCIETY
LA English
DT Meeting Abstract
CT 245th National Meeting of the American-Chemical-Society (ACS)
CY APR 07-11, 2013
CL New Orleans, LA
SP Amer Chem Soc
C1 [Rajput, Nav N.; Hung, Francisco R.] Louisiana State Univ, Cain Dept Chem Engn, Baton Rouge, LA 70803 USA.
[Monk, Joshua] NASA, Thermal Protect Mat Branch, Ames Res Ctr, Moffett Field, CA 94035 USA.
EM nrajpu1@tigers.lsu.edu
NR 0
TC 0
Z9 0
U1 0
U2 1
PU AMER CHEMICAL SOC
PI WASHINGTON
PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA
SN 0065-7727
J9 ABSTR PAP AM CHEM S
JI Abstr. Pap. Am. Chem. Soc.
PD APR 7
PY 2013
VL 245
MA 449-COMP
PG 1
WC Chemistry, Multidisciplinary
SC Chemistry
GA 210RD
UT WOS:000323851304444
ER
PT J
AU Rajput, NN
Monk, J
Singh, R
Hung, FR
AF Rajput, Nav N.
Monk, Joshua
Singh, Ramesh
Hung, Francisco R.
TI Molecular modeling of the ionic liquid [EMIM+][TFMSI-] confined in model
nanoporous materials
SO ABSTRACTS OF PAPERS OF THE AMERICAN CHEMICAL SOCIETY
LA English
DT Meeting Abstract
CT 245th National Meeting of the American-Chemical-Society (ACS)
CY APR 07-11, 2013
CL New Orleans, LA
SP Amer Chem Soc
C1 [Rajput, Nav N.; Hung, Francisco R.] Louisiana State Univ, Cain Dept Chem Engn, Baton Rouge, LA 70803 USA.
[Monk, Joshua] NASA, Thermal Protect Mat Branch, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Singh, Ramesh] Univ Notre Dame, Dept Chem & Biomol Engn, Notre Dame, IN 46556 USA.
EM nrajpu1@tigers.lsu.edu
NR 0
TC 0
Z9 0
U1 0
U2 1
PU AMER CHEMICAL SOC
PI WASHINGTON
PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA
SN 0065-7727
J9 ABSTR PAP AM CHEM S
JI Abstr. Pap. Am. Chem. Soc.
PD APR 7
PY 2013
VL 245
MA 240-COMP
PG 1
WC Chemistry, Multidisciplinary
SC Chemistry
GA 210RD
UT WOS:000323851304267
ER
PT J
AU Sutton, AJ
McKenzie, K
Ware, B
de Vine, G
Spero, RE
Klipstein, W
Shaddock, DA
AF Sutton, Andrew J.
McKenzie, Kirk
Ware, Brent
de Vine, Glenn
Spero, Robert E.
Klipstein, W.
Shaddock, Daniel A.
TI Improved optical ranging for space based gravitational wave detection
SO CLASSICAL AND QUANTUM GRAVITY
LA English
DT Article
ID LISA; LASER; COMMUNICATION
AB The operation of 10(6) km scale laser interferometers in space will permit the detection of gravitational waves at previously unaccessible frequency regions. Multi-spacecraft missions, such as the Laser Interferometer Space Antenna (LISA), will use time delay interferometry to suppress the otherwise dominant laser frequency noise from their measurements. This is accomplished by performing sub-sample interpolation of the optical phase measurements recorded at each spacecraft for synchronization and cancellation of the otherwise dominant laser frequency noise. These sub-sample interpolation time shifts are dependent upon the inter-spacecraft range and will be measured using a pseudo-random noise ranging modulation upon the science laser. One limit to the ranging performance is mutual interference between the outgoing and incoming ranging signals upon each spacecraft. This paper reports on the demonstration of a noise cancellation algorithm which is shown to providing a factor of similar to 8 suppression of the mutual interference noise. Demonstration of the algorithm in an optical test bed showed an rms ranging error of 0.06 m, improved from 0.19 m in previous results, surpassing the 1 m RMS LISA specification and potentially improving the cancellation of laser frequency noise.
C1 [Sutton, Andrew J.; Shaddock, Daniel A.] Australian Natl Univ, Ctr Gravitat Phys, Canberra, ACT 0200, Australia.
[McKenzie, Kirk; Ware, Brent; de Vine, Glenn; Spero, Robert E.; Klipstein, W.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Sutton, AJ (reprint author), Australian Natl Univ, Ctr Gravitat Phys, GPO Box 4, Canberra, ACT 0200, Australia.
EM andrew.sutton@anu.edu.au
RI Shaddock, Daniel/A-7534-2011
OI Shaddock, Daniel/0000-0002-6885-3494
NR 25
TC 4
Z9 4
U1 2
U2 12
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0264-9381
J9 CLASSICAL QUANT GRAV
JI Class. Quantum Gravity
PD APR 7
PY 2013
VL 30
IS 7
AR 075008
DI 10.1088/0264-9381/30/7/075008
PG 8
WC Astronomy & Astrophysics; Physics, Multidisciplinary; Physics, Particles
& Fields
SC Astronomy & Astrophysics; Physics
GA 107OK
UT WOS:000316227500008
ER
PT J
AU Aguilar, M
Alberti, G
Alpat, B
Alvino, A
Ambrosi, G
Andeen, K
Anderhub, H
Arruda, L
Azzarello, P
Bachlechner, A
Barao, F
Baret, B
Barrau, A
Barrin, L
Bartoloni, A
Basara, L
Basili, A
Batalha, L
Bates, J
Battiston, R
Bazo, J
Becker, R
Becker, U
Behlmann, M
Beischer, B
Berdugo, J
Berges, P
Bertucci, B
Bigongiari, G
Biland, A
Bindi, V
Bizzaglia, S
Boella, G
de Boer, W
Bollweg, K
Bolmont, J
Borgia, B
Borsini, S
Boschini, MJ
Boudoul, G
Bourquin, M
Brun, P
Buenerd, M
Burger, J
Burger, W
Cadoux, F
Cai, XD
Capell, M
Casadei, D
Casaus, J
Cascioli, V
Castellini, G
Cernuda, I
Cervelli, F
Chae, MJ
Chang, YH
Chen, AI
Chen, CR
Chen, H
Cheng, GM
Chen, HS
Cheng, L
Chernoplyiokov, N
Chikanian, A
Choumilov, E
Choutko, V
Chung, CH
Clark, C
Clavero, R
Coignet, G
Commichau, V
Consolandi, C
Contin, A
Corti, C
Dios, MTC
Coste, B
Crespo, D
Cui, Z
Dai, M
Delgado, C
Della Torre, S
Demirkoz, B
Dennett, P
Derome, L
Di Falco, S
Diao, XH
Diago, A
Djambazov, L
Diaz, C
von Doetinchem, P
Du, WJ
Dubois, JM
Duperay, R
Duranti, M
D'Urso, D
Egorov, A
Eline, A
Eppling, FJ
Eronen, T
van Es, J
Esser, H
Falvard, A
Fiandrini, E
Fiasson, A
Finch, E
Fisher, P
Flood, K
Foglio, R
Fohey, M
Fopp, S
Fouque, N
Galaktionov, Y
Gallilee, M
Gallin-Martel, L
Gallucci, G
Garcia, B
Garcia, J
Garcia-Lopez, R
Garcia-Tabares, L
Gargiulo, C
Gast, H
Gebauer, I
Gentile, S
Gervasi, M
Gillard, W
Giovacchini, F
Girard, L
Goglov, P
Gong, J
Goy-Henningsen, C
Grandi, D
Graziani, M
Grechko, A
Gross, A
Guerri, I
de la Guia, C
Guo, KH
Habiby, M
Haino, S
Hauler, F
He, ZH
Heil, M
Heilig, J
Hermel, R
Hofer, H
Huang, ZC
Hungerford, W
Incagli, M
Ionica, M
Jacholkowska, A
Jang, WY
Jinchi, H
Jongmanns, M
Journet, L
Jungermann, L
Karpinski, W
Kim, GN
Kim, KS
Kirn, T
Kossakowski, R
Koulemzine, A
Kounina, O
Kounine, A
Koutsenko, V
Krafczyk, MS
Laudi, E
Laurenti, G
Lauritzen, C
Lebedev, A
Lee, MW
Lee, SC
Leluc, C
Vargas, HL
Lepareur, V
Li, JQ
Li, Q
Li, TX
Li, W
Li, ZH
Lipari, P
Lin, CH
Liu, D
Liu, H
Lomtadze, T
Lu, YS
Lucidi, S
Lubelsmeyer, K
Luo, JZ
Lustermann, W
Lv, S
Madsen, J
Majka, R
Malinin, A
Mana, C
Marin, J
Martin, T
Martinez, G
Masciocchi, F
Masi, N
Maurin, D
McInturff, A
McIntyre, P
Menchaca-Rocha, A
Meng, Q
Menichelli, M
Mereu, I
Millinger, M
Mo, DC
Molina, M
Mott, P
Mujunen, A
Natale, S
Nemeth, P
Ni, JQ
Nikonov, N
Nozzoli, F
Nunes, P
Obermeier, A
Oh, S
Oliva, A
Palmonari, F
Palomares, C
Paniccia, M
Papi, A
Park, WH
Pauluzzi, M
Pauss, F
Pauw, A
Pedreschi, E
Pensotti, S
Pereira, R
Perrin, E
Pessina, G
Pierschel, G
Pilo, F
Piluso, A
Pizzolotto, C
Plyaskin, V
Pochon, J
Pohl, M
Poireau, V
Porter, S
Pouxe, J
Putze, A
Quadrani, L
Qi, XN
Rancoita, PG
Rapin, D
Ren, ZL
Ricol, JS
Riihonen, E
Rodriguez, I
Roeser, U
Rosier-Lees, S
Rossi, L
Rozhkov, A
Rozza, D
Sabellek, A
Sagdeev, R
Sandweiss, J
Santos, B
Saouter, P
Sarchioni, M
Schael, S
Schinzel, D
Schmanau, M
Schwering, G
von Dratzig, AS
Scolieri, G
Seo, ES
Shan, BS
Shi, JY
Shi, YM
Siedenburg, T
Siedling, R
Son, D
Spada, F
Spinella, F
Steuer, M
Stiff, K
Sun, W
Sun, WH
Sun, XH
Tacconi, M
Tang, CP
Tang, XW
Tang, ZC
Tao, L
Tassan-Viol, J
Ting, SCC
Ting, SM
Titus, C
Tomassetti, N
Toral, F
Torsti, J
Tsai, JR
Tutt, JC
Ulbricht, J
Urban, T
Vagelli, V
Valente, E
Vannini, C
Valtonen, E
Trevino, MV
Vaurynovich, S
Vecchi, M
Vergain, M
Verlaat, B
Vescovi, C
Vialle, JP
Viertel, G
Volpini, G
Wang, D
Wang, NH
Wang, QL
Wang, RS
Wang, X
Wang, ZX
Wallraff, W
Weng, ZL
Willenbrock, M
Wlochal, M
Wu, H
Wu, KY
Wu, ZS
Xiao, WJ
Xie, S
Xiong, RQ
Xin, GM
Xu, NS
Xu, W
Yan, Q
Yang, J
Yang, M
Ye, QH
Yi, H
Yu, YJ
Yu, ZQ
Zeissler, S
Zhang, JG
Zhang, Z
Zhang, MM
Zheng, ZM
Zhuang, HL
Zhukov, V
Zichichi, A
Zuccon, P
Zurbach, C
AF Aguilar, M.
Alberti, G.
Alpat, B.
Alvino, A.
Ambrosi, G.
Andeen, K.
Anderhub, H.
Arruda, L.
Azzarello, P.
Bachlechner, A.
Barao, F.
Baret, B.
Barrau, A.
Barrin, L.
Bartoloni, A.
Basara, L.
Basili, A.
Batalha, L.
Bates, J.
Battiston, R.
Bazo, J.
Becker, R.
Becker, U.
Behlmann, M.
Beischer, B.
Berdugo, J.
Berges, P.
Bertucci, B.
Bigongiari, G.
Biland, A.
Bindi, V.
Bizzaglia, S.
Boella, G.
de Boer, W.
Bollweg, K.
Bolmont, J.
Borgia, B.
Borsini, S.
Boschini, M. J.
Boudoul, G.
Bourquin, M.
Brun, P.
Buenerd, M.
Burger, J.
Burger, W.
Cadoux, F.
Cai, X. D.
Capell, M.
Casadei, D.
Casaus, J.
Cascioli, V.
Castellini, G.
Cernuda, I.
Cervelli, F.
Chae, M. J.
Chang, Y. H.
Chen, A. I.
Chen, C. R.
Chen, H.
Cheng, G. M.
Chen, H. S.
Cheng, L.
Chernoplyiokov, N.
Chikanian, A.
Choumilov, E.
Choutko, V.
Chung, C. H.
Clark, C.
Clavero, R.
Coignet, G.
Commichau, V.
Consolandi, C.
Contin, A.
Corti, C.
Dios, M. T. Costado
Coste, B.
Crespo, D.
Cui, Z.
Dai, M.
Delgado, C.
Della Torre, S.
Demirkoz, B.
Dennett, P.
Derome, L.
Di Falco, S.
Diao, X. H.
Diago, A.
Djambazov, L.
Diaz, C.
von Doetinchem, P.
Du, W. J.
Dubois, J. M.
Duperay, R.
Duranti, M.
D'Urso, D.
Egorov, A.
Eline, A.
Eppling, F. J.
Eronen, T.
van Es, J.
Esser, H.
Falvard, A.
Fiandrini, E.
Fiasson, A.
Finch, E.
Fisher, P.
Flood, K.
Foglio, R.
Fohey, M.
Fopp, S.
Fouque, N.
Galaktionov, Y.
Gallilee, M.
Gallin-Martel, L.
Gallucci, G.
Garcia, B.
Garcia, J.
Garcia-Lopez, R.
Garcia-Tabares, L.
Gargiulo, C.
Gast, H.
Gebauer, I.
Gentile, S.
Gervasi, M.
Gillard, W.
Giovacchini, F.
Girard, L.
Goglov, P.
Gong, J.
Goy-Henningsen, C.
Grandi, D.
Graziani, M.
Grechko, A.
Gross, A.
Guerri, I.
de la Guia, C.
Guo, K. H.
Habiby, M.
Haino, S.
Hauler, F.
He, Z. H.
Heil, M.
Heilig, J.
Hermel, R.
Hofer, H.
Huang, Z. C.
Hungerford, W.
Incagli, M.
Ionica, M.
Jacholkowska, A.
Jang, W. Y.
Jinchi, H.
Jongmanns, M.
Journet, L.
Jungermann, L.
Karpinski, W.
Kim, G. N.
Kim, K. S.
Kirn, Th.
Kossakowski, R.
Koulemzine, A.
Kounina, O.
Kounine, A.
Koutsenko, V.
Krafczyk, M. S.
Laudi, E.
Laurenti, G.
Lauritzen, C.
Lebedev, A.
Lee, M. W.
Lee, S. C.
Leluc, C.
Vargas, H. Leon
Lepareur, V.
Li, J. Q.
Li, Q.
Li, T. X.
Li, W.
Li, Z. H.
Lipari, P.
Lin, C. H.
Liu, D.
Liu, H.
Lomtadze, T.
Lu, Y. S.
Lucidi, S.
Luebelsmeyer, K.
Luo, J. Z.
Lustermann, W.
Lv, S.
Madsen, J.
Majka, R.
Malinin, A.
Mana, C.
Marin, J.
Martin, T.
Martinez, G.
Masciocchi, F.
Masi, N.
Maurin, D.
McInturff, A.
McIntyre, P.
Menchaca-Rocha, A.
Meng, Q.
Menichelli, M.
Mereu, I.
Millinger, M.
Mo, D. C.
Molina, M.
Mott, P.
Mujunen, A.
Natale, S.
Nemeth, P.
Ni, J. Q.
Nikonov, N.
Nozzoli, F.
Nunes, P.
Obermeier, A.
Oh, S.
Oliva, A.
Palmonari, F.
Palomares, C.
Paniccia, M.
Papi, A.
Park, W. H.
Pauluzzi, M.
Pauss, F.
Pauw, A.
Pedreschi, E.
Pensotti, S.
Pereira, R.
Perrin, E.
Pessina, G.
Pierschel, G.
Pilo, F.
Piluso, A.
Pizzolotto, C.
Plyaskin, V.
Pochon, J.
Pohl, M.
Poireau, V.
Porter, S.
Pouxe, J.
Putze, A.
Quadrani, L.
Qi, X. N.
Rancoita, P. G.
Rapin, D.
Ren, Z. L.
Ricol, J. S.
Riihonen, E.
Rodriguez, I.
Roeser, U.
Rosier-Lees, S.
Rossi, L.
Rozhkov, A.
Rozza, D.
Sabellek, A.
Sagdeev, R.
Sandweiss, J.
Santos, B.
Saouter, P.
Sarchioni, M.
Schael, S.
Schinzel, D.
Schmanau, M.
Schwering, G.
von Dratzig, A. Schulz
Scolieri, G.
Seo, E. S.
Shan, B. S.
Shi, J. Y.
Shi, Y. M.
Siedenburg, T.
Siedling, R.
Son, D.
Spada, F.
Spinella, F.
Steuer, M.
Stiff, K.
Sun, W.
Sun, W. H.
Sun, X. H.
Tacconi, M.
Tang, C. P.
Tang, X. W.
Tang, Z. C.
Tao, L.
Tassan-Viol, J.
Ting, Samuel C. C.
Ting, S. M.
Titus, C.
Tomassetti, N.
Toral, F.
Torsti, J.
Tsai, J. R.
Tutt, J. C.
Ulbricht, J.
Urban, T.
Vagelli, V.
Valente, E.
Vannini, C.
Valtonen, E.
Trevino, M. Vargas
Vaurynovich, S.
Vecchi, M.
Vergain, M.
Verlaat, B.
Vescovi, C.
Vialle, J. P.
Viertel, G.
Volpini, G.
Wang, D.
Wang, N. H.
Wang, Q. L.
Wang, R. S.
Wang, X.
Wang, Z. X.
Wallraff, W.
Weng, Z. L.
Willenbrock, M.
Wlochal, M.
Wu, H.
Wu, K. Y.
Wu, Z. S.
Xiao, W. J.
Xie, S.
Xiong, R. Q.
Xin, G. M.
Xu, N. S.
Xu, W.
Yan, Q.
Yang, J.
Yang, M.
Ye, Q. H.
Yi, H.
Yu, Y. J.
Yu, Z. Q.
Zeissler, S.
Zhang, J. G.
Zhang, Z.
Zhang, M. M.
Zheng, Z. M.
Zhuang, H. L.
Zhukov, V.
Zichichi, A.
Zuccon, P.
Zurbach, C.
CA AMS Collaboration
TI First Result from the Alpha Magnetic Spectrometer on the International
Space Station: Precision Measurement of the Positron Fraction in Primary
Cosmic Rays of 0.5-350 GeV
SO PHYSICAL REVIEW LETTERS
LA English
DT Article
ID AMS RICH DETECTOR; TIME-OF-FLIGHT; FAST TRIGGER; IDENTIFICATION;
PROTOTYPE; ELECTRONS; EARTH; TRD
AB A precision measurement by the Alpha Magnetic Spectrometer on the International Space Station of the positron fraction in primary cosmic rays in the energy range from 0.5 to 350 GeV based on 6.8 x 10(6) positron and electron events is presented. The very accurate data show that the positron fraction is steadily increasing from 10 to similar to 250 GeV, but, from 20 to 250 GeV, the slope decreases by an order of magnitude. The positron fraction spectrum shows no fine structure, and the positron to electron ratio shows no observable anisotropy. Together, these features show the existence of new physical phenomena. DOI: 10.1103/PhysRevLett.110.141102
C1 [Basili, A.; Becker, R.; Becker, U.; Behlmann, M.; Berges, P.; Burger, J.; Cai, X. D.; Capell, M.; Chen, A. I.; Chen, H.; Choumilov, E.; Choutko, V.; Dennett, P.; Egorov, A.; Eline, A.; Eppling, F. J.; Fisher, P.; Flood, K.; Galaktionov, Y.; Gallilee, M.; Gargiulo, C.; Goglov, P.; Hungerford, W.; Incagli, M.; Koulemzine, A.; Kounina, O.; Kounine, A.; Koutsenko, V.; Krafczyk, M. S.; Lebedev, A.; Plyaskin, V.; Rozhkov, A.; Schinzel, D.; Steuer, M.; Sun, W.; Ting, Samuel C. C.; Ting, S. M.; Titus, C.; Vaurynovich, S.; Vergain, M.; Wang, X.; Willenbrock, M.; Zuccon, P.] Rhein Westfal TH Aachen, Phys Inst B, D-52056 Aachen, Germany.
[Madsen, J.] Univ Aarhus, Dept Phys & Astron, DK-8000 Aarhus C, Denmark.
[Verlaat, B.] NIKHEF, Natl Inst Nucl Phys & High Energy Phys, NL-1098 SJ Amsterdam, Netherlands.
[Demirkoz, B.] Middle E Tech Univ, Dept Phys, TR-06800 Ankara, Turkey.
[Basara, L.; Brun, P.; Cadoux, F.; Coignet, G.; Dubois, J. M.; Fiasson, A.; Fouque, N.; Girard, L.; Goy-Henningsen, C.; Hermel, R.; Journet, L.; Kossakowski, R.; Lepareur, V.; Paniccia, M.; Pochon, J.; Poireau, V.; Rosier-Lees, S.; Tao, L.; Tassan-Viol, J.; Vialle, J. P.] CNRS, LAPP, IN2P3, Lab Annecy Le Vieux Phys Particules, F-74941 Annecy Le Vieux, France.
[Basara, L.; Brun, P.; Cadoux, F.; Coignet, G.; Dubois, J. M.; Fiasson, A.; Fouque, N.; Girard, L.; Goy-Henningsen, C.; Hermel, R.; Journet, L.; Kossakowski, R.; Lepareur, V.; Paniccia, M.; Pochon, J.; Poireau, V.; Rosier-Lees, S.; Tao, L.; Tassan-Viol, J.; Vialle, J. P.] Univ Savoie, F-74941 Annecy Le Vieux, France.
[Li, W.; Shan, B. S.; Wu, K. Y.; Zheng, Z. M.] Beihang Univ, BUAA, Beijing 100191, Peoples R China.
[Dai, M.; Wang, Q. L.; Yu, Y. J.] Chinese Acad Sci, Inst Elect Engn, IEE, Beijing 100080, Peoples R China.
[Cheng, G. M.; Chen, H. S.; Li, Z. H.; Lu, Y. S.; Tang, X. W.; Tang, Z. C.; Xu, W.; Yan, Q.; Yang, M.; Yu, Z. Q.; Zhuang, H. L.] Chinese Acad Sci, Inst High Energy Phys, IHEP, Beijing 100039, Peoples R China.
[Casadei, D.; Contin, A.; Laurenti, G.; Masi, N.; Palmonari, F.; Quadrani, L.; Zichichi, A.] INFN Sez Bologna, I-40126 Bologna, Italy.
[Casadei, D.; Contin, A.; Masi, N.; Palmonari, F.; Quadrani, L.; Zichichi, A.] Univ Bologna, I-40126 Bologna, Italy.
[Basili, A.; Becker, R.; Becker, U.; Behlmann, M.; Berges, P.; Burger, J.; Cai, X. D.; Capell, M.; Chen, A. I.; Chen, H.; Choumilov, E.; Choutko, V.; Dennett, P.; Egorov, A.; Eline, A.; Eppling, F. J.; Fisher, P.; Flood, K.; Galaktionov, Y.; Gallilee, M.; Gargiulo, C.; Goglov, P.; Hungerford, W.; Incagli, M.; Koulemzine, A.; Kounina, O.; Kounine, A.; Koutsenko, V.; Krafczyk, M. S.; Lebedev, A.; Plyaskin, V.; Rozhkov, A.; Schinzel, D.; Steuer, M.; Sun, W.; Ting, Samuel C. C.; Ting, S. M.; Titus, C.; Vaurynovich, S.; Vergain, M.; Wang, X.; Willenbrock, M.; Zuccon, P.] MIT, Cambridge, MA 02139 USA.
[Chang, Y. H.; Haino, S.; Vecchi, M.] Natl Cent Univ, Tao Yuan 32054, Taiwan.
[Sagdeev, R.] Univ Maryland, East West Ctr Space Sci, College Pk, MD 20742 USA.
[Malinin, A.; Seo, E. S.] Univ Maryland, IPST, College Pk, MD 20742 USA.
[McInturff, A.; McIntyre, P.; Stiff, K.] Texas A&M Univ, Dept Phys, College Stn, TX 77843 USA.
[Jang, W. Y.; Kim, G. N.; Kim, K. S.; Lee, M. W.; Park, W. H.; Son, D.] Kyungpook Natl Univ, CHEP, Taegu 702701, South Korea.
[van Es, J.; Pauw, A.] NLR, Natl Aerosp Lab, NL-8300 AD Emmeloord, Netherlands.
[Castellini, G.] CNR IROE, I-50125 Florence, Italy.
[Nozzoli, F.; Pizzolotto, C.] ASDC ESRIN, I-00044 Frascati, Italy.
[Aguilar, M.; Barrin, L.; D'Urso, D.; Rossi, L.; Rozza, D.] CERN, European Org Nucl Res, CH-1211 Geneva 23, Switzerland.
[Azzarello, P.; Bourquin, M.; Cadoux, F.; Habiby, M.; Leluc, C.; Masciocchi, F.; Paniccia, M.; Perrin, E.; Pohl, M.; Rapin, D.; Saouter, P.] Univ Geneva, DPNC, CH-1211 Geneva 4, Switzerland.
[Baret, B.; Barrau, A.; Boudoul, G.; Buenerd, M.; Coste, B.; Derome, L.; Duperay, R.; Foglio, R.; Gallin-Martel, L.; Gillard, W.; Maurin, D.; Pouxe, J.; Ricol, J. S.; Trevino, M. Vargas; Vescovi, C.] CNRS, LPSC, IN2P3, F-38026 St Martin Dheres, France.
[Alvino, A.; Baret, B.; Barrau, A.; Boudoul, G.; Buenerd, M.; Coste, B.; Derome, L.; Duperay, R.; Foglio, R.; Gallin-Martel, L.; Gillard, W.; Maurin, D.; Pouxe, J.; Ricol, J. S.; Trevino, M. Vargas; Vescovi, C.] Univ Grenoble 1, Grenoble INP, F-38026 Grenoble, France.
[Diao, X. H.; Guo, K. H.; He, Z. H.; Huang, Z. C.; Li, T. X.; Lv, S.; Mo, D. C.; Ni, J. Q.; Qi, X. N.; Sun, X. H.; Tang, C. P.; Wang, Z. X.; Weng, Z. L.; Wu, Z. S.; Xiao, W. J.; Xu, N. S.; Zhang, Z.; Zhang, M. M.] Sun Yat Sen Univ, Guangzhou 510275, Peoples R China.
[Bindi, V.; Consolandi, C.; Corti, C.] Univ Hawaii, Dept Phys & Astron, Honolulu, HI 96822 USA.
[Bates, J.; Bollweg, K.; Clark, C.; Fohey, M.; Heilig, J.; Hungerford, W.; Lauritzen, C.; Martin, T.; Mott, P.; Nemeth, P.; Porter, S.; Tutt, J. C.; Urban, T.] NASA, Johnson Space Ctr, JSC, Houston, TX 77058 USA.
[Bates, J.; Bollweg, K.; Clark, C.; Fohey, M.; Heilig, J.; Hungerford, W.; Lauritzen, C.; Martin, T.; Mott, P.; Nemeth, P.; Porter, S.; Tutt, J. C.; Urban, T.] Jacobs Sverdrup, Houston, TX 77058 USA.
[Chen, C. R.; Tsai, J. R.; Wang, D.] Natl Space Org, Hsinchu 300, Taiwan.
[Mujunen, A.] Aalto Univ, Metsahovi Radio Observ, FIN-02540 Kylmala, Finland.
[Andeen, K.; de Boer, W.; Gebauer, I.; Hauler, F.; Heil, M.; Jungermann, L.; Nikonov, N.; Obermeier, A.; Sabellek, A.; Schmanau, M.; Vagelli, V.; Zeissler, S.] Karlsruhe Inst Technol, Inst Expt Kernphys, D-76128 Karlsruhe, Germany.
[Clavero, R.; Dios, M. T. Costado; Diago, A.; Garcia-Lopez, R.; Pochon, J.] Inst Astrofis Canarias, E-38205 Tenerife, Spain.
[Arruda, L.; Barao, F.; Batalha, L.; Nunes, P.; Pereira, R.; Santos, B.] LIP, Lab Instrumentacao & Fis Expt Particulas, P-1000 Lisbon, Portugal.
[Jinchi, H.] Chung Shan Inst Sci & Technol, Tao Yuan 325, Taiwan.
[Aguilar, M.; Berdugo, J.; Casaus, J.; Cernuda, I.; Crespo, D.; Delgado, C.; Diaz, C.; Garcia, B.; Garcia, J.; Garcia-Tabares, L.; Giovacchini, F.; de la Guia, C.; Mana, C.; Marin, J.; Martinez, G.; Oliva, A.; Palomares, C.; Rodriguez, I.; Toral, F.] CIEMAT, Ctr Invest Energet Medioambientales & Tecnol, E-28040 Madrid, Spain.
[Vargas, H. Leon; Menchaca-Rocha, A.] Univ Nacl Autonoma Mexico, Inst Fis, Mexico City 01000, DF, Mexico.
[Volpini, G.] INFN Sez Milano, I-20090 Milan, Italy.
[Rossi, L.; Volpini, G.] Univ Milan, I-20090 Milan, Italy.
[Boella, G.; Boschini, M. J.; Consolandi, C.; Della Torre, S.; Gervasi, M.; Grandi, D.; Pensotti, S.; Pessina, G.; Rancoita, P. G.; Rozza, D.; Tacconi, M.] INFN Sez Milano Bicocca, I-20126 Milan, Italy.
[Boella, G.; Della Torre, S.; Gervasi, M.; Pensotti, S.; Pessina, G.; Rozza, D.; Tacconi, M.] Univ Milano Bicocca, I-20126 Milan, Italy.
[Bolmont, J.; Falvard, A.; Jacholkowska, A.; Zurbach, C.] CNRS, IN2P3, LUPM Ex LPTA, Lab Univ & Particules Montpellier, F-34095 Montpellier, France.
[Bolmont, J.; Falvard, A.; Jacholkowska, A.; Zurbach, C.] Univ Montpellier 2, F-34095 Montpellier, France.
[Chernoplyiokov, N.; Grechko, A.] Russian Res Ctr, Kurchatov Inst, Moscow 123182, Russia.
[Gong, J.; Li, J. Q.; Li, Q.; Liu, H.; Luo, J. Z.; Meng, Q.; Shi, J. Y.; Sun, W. H.; Wu, H.; Xiong, R. Q.; Yi, H.; Zhang, J. G.] Southeast Univ, SEU, Nanjing 210096, Jiangsu, Peoples R China.
[Chikanian, A.; Finch, E.; Majka, R.; Sandweiss, J.] Yale Univ, Dept Phys, New Haven, CT 06520 USA.
[Alberti, G.; Alpat, B.; Alvino, A.; Ambrosi, G.; Azzarello, P.; Battiston, R.; Bazo, J.; Bertucci, B.; Bizzaglia, S.; Borsini, S.; Cascioli, V.; Duranti, M.; D'Urso, D.; Fiandrini, E.; Graziani, M.; Haino, S.; Ionica, M.; Laudi, E.; Lucidi, S.; Menichelli, M.; Mereu, I.; Nozzoli, F.; Oliva, A.; Papi, A.; Pauluzzi, M.; Piluso, A.; Pizzolotto, C.; Sarchioni, M.; Scolieri, G.; Tomassetti, N.; Zuccon, P.] INFN Sez Perugia, I-06100 Perugia, Italy.
[Alberti, G.; Alvino, A.; Battiston, R.; Bertucci, B.; Borsini, S.; Burger, W.; Cascioli, V.; Duranti, M.; Fiandrini, E.; Graziani, M.; Ionica, M.; Laudi, E.; Mereu, I.; Oliva, A.; Pauluzzi, M.; Piluso, A.; Tomassetti, N.] Univ Perugia, I-06100 Perugia, Italy.
[Bigongiari, G.; Cervelli, F.; Di Falco, S.; Gallucci, G.; Guerri, I.; Incagli, M.; Lomtadze, T.; Pedreschi, E.; Pilo, F.; Spinella, F.; Vannini, C.] INFN Sez Pisa, I-56100 Pisa, Italy.
[Bigongiari, G.; Guerri, I.] Univ Pisa, I-56100 Pisa, Italy.
[Battiston, R.] INFN TIFPA, I-38123 Povo, Trento, Italy.
[Battiston, R.] Univ Trent, I-38123 Povo, Trento, Italy.
[Bartoloni, A.; Borgia, B.; Gargiulo, C.; Gentile, S.; Lipari, P.; Spada, F.; Valente, E.] INFN Sez Roma 1, I-00185 Rome, Italy.
[Borgia, B.; Gentile, S.] Univ Roma La Sapienza, I-00185 Rome, Italy.
[Chae, M. J.; Oh, S.; Yang, J.] Ewha Womans Univ, Dept Phys, Seoul 120750, South Korea.
[Cheng, L.; Cui, Z.; Du, W. J.; Wang, N. H.; Xin, G. M.] Shandong Univ, SDU, Jinan 51, Shandong, Peoples R China.
[Shi, Y. M.; Wang, R. S.; Xie, S.; Ye, Q. H.] Shanghai Jiao Tong Univ, SJTU, Shanghai 200030, Peoples R China.
[Lee, S. C.; Lin, C. H.; Liu, D.; Natale, S.; Ren, Z. L.; Weng, Z. L.; Wu, K. Y.] Acad Sinica, Inst Phys, Taipei 11529, Taiwan.
[Eronen, T.; Riihonen, E.; Torsti, J.; Valtonen, E.] Univ Turku, Dept Phys, Space Res Lab, FIN-20014 Turku, Finland.
[Anderhub, H.; Biland, A.; Commichau, V.; Djambazov, L.; Hofer, H.; Jongmanns, M.; Lustermann, W.; Pauss, F.; Roeser, U.; Ulbricht, J.; Viertel, G.] ETH, Inst Particle Phys, CH-8093 Zurich, Switzerland.
RP Aguilar, M (reprint author), CIEMAT, Ctr Invest Energet Medioambientales & Tecnol, E-28040 Madrid, Spain.
RI Zuccon, Paolo/I-7736-2012; Ye, Qinghao/O-5630-2015; Palomares,
Carmen/H-7783-2015; Duranti, Matteo/I-7691-2013; Tomassetti,
Nicola/K-2380-2016; Masi, Nicolo/G-7911-2016; Pizzolotto,
Cecilia/G-5821-2013; Barao, Fernando/O-2357-2016; Paniccia,
Mercedes/A-4519-2017; alpat, ali behcet/G-6290-2013; Delgado,
Carlos/K-7587-2014; Rancoita, Pier Giorgio/J-9896-2015; Fiandrini,
Emanuele/C-4549-2008; bertucci, bruna/J-5237-2012; Casadei,
Diego/I-1785-2013; Zhukov, Valery/K-3615-2013; Arruda,
Luisa/I-2403-2013; Vecchi, Manuela/J-9180-2014; Martinez Botella,
Gustavo/K-8834-2014; Marin, Jesus/K-6991-2014; Berdugo,
Javier/A-2858-2015; Demirkoz, Bilge/C-8179-2014;
OI Zuccon, Paolo/0000-0002-2728-0167; Palomares,
Carmen/0000-0003-4374-9065; Duranti, Matteo/0000-0003-0980-6425;
Tomassetti, Nicola/0000-0002-0856-9299; Masi,
Nicolo/0000-0002-3729-7608; Pizzolotto, Cecilia/0000-0003-0200-2408;
Barao, Fernando/0000-0002-8346-9941; Paniccia,
Mercedes/0000-0001-8482-2703; alpat, ali behcet/0000-0002-0116-1506;
Delgado, Carlos/0000-0002-7014-4101; Rancoita, Pier
Giorgio/0000-0002-1990-4283; Arruda, Luisa/0000-0001-6720-6933; Martinez
Botella, Gustavo/0000-0002-1061-8520; Marin, Jesus/0000-0002-9049-3667;
Berdugo, Javier/0000-0002-7911-8532; Della Torre,
Stefano/0000-0002-7669-0859; Seo, Eun-Suk/0000-0001-8682-805X; Casadei,
Diego/0000-0002-3343-3529; Vagelli, Valerio/0000-0002-4495-9331; Basara,
Laurent/0000-0002-5726-9954; PAPI, ALBERTO/0000-0002-6924-4500; Corti,
Claudio/0000-0001-9127-7133; Bertucci, Bruna/0000-0001-7584-293X;
Graziani, Maura/0000-0001-7570-2048; Pessina, Gianluigi
Ezio/0000-0003-3700-9757; Tacconi, Mauro/0000-0002-9344-6305; Nozzoli,
Francesco/0000-0002-4355-7947; Ambrosi, Giovanni/0000-0001-6977-9559;
Castellini, Guido/0000-0002-0177-0643; Rozza,
Davide/0000-0002-7378-6353; Bigongiari, Gabriele/0000-0003-3691-0826;
GILLARD, William/0000-0003-4744-9748; Quadrani,
Lucio/0000-0003-4830-0259; Gallucci, Giovanni/0000-0003-3554-9733
FU U.S. DOE; CERN; Deutsches Zentrum fur Luft- und Raumfahrt, DLR; National
Natural Science Foundation of China; Italian Space Agency, ASI; SEIDI;
CPAN
FX We thank former NASA Administrator Daniel S. Goldin for his dedication
to the legacy of the ISS as a scientific laboratory and his decision for
NASA to fly AMS as a DOE payload. We also acknowledge the continuous
support of the current and former NASA leadership including Charles
Bolden, Lori Garver, William Gerstenmeier, George Abbey, Franklin
Chang-Diaz, and Mark Sistilli, and we thank the crew of STS-134: Mark
Kelly, Greg Johnson, Greg Chamitoff, Drew Feustel, Mike Fincke, and
Roberto Vittori. AMS is a U.S. DOE sponsored international
collaboration. We are grateful for the support of Jim Siegrist, Michael
Salamon, Dennis Kovar, Robin Staffin, Saul Gonzalez, and John O'Fallon.
We also acknowledge the continuous support from MIT, beginning with
former President Charles M. Vest, and its School of Science, Marc
Kastner, Robert Silbey, Robert Birgeneau, Ernest Moniz, Edmund
Bertschinger, and Richard Milner. We acknowledge support from CAS, NNSF,
MOST, NLAA, and the Provincial Governments of Shandong, Jiangsu, and
Guandong, China; CNRS, IN2P3, CNES, Enigmass, and the ANR, France, and
Bernard Accoyer, former President of the French National Assembly; DLR,
the Julich Supercomputing Center, P. Hintze, J. Trumper, and J. D.
Woerner, Germany; INFN, ASI, E. Iarocci, R. Petronzio, F. Ferroni, S. De
Julio, S. Vetrella, G. Bignami, and E. Saggese, Italy; CIEMAT, CDTI,
SEIDI-MINECO, and CPAN, Spain; the Swiss National Science Foundation
(SNSF), federal and cantonal authorities, Switzerland; and Academia
Sinica and the National Science Council (NSC), former President of
Academia Sinica Yuan-Tseh Lee and former Ministers of NSC Chien-Jen
Chen, Maw-Kuen Wu, and Luo-Chuan Lee, Taiwan. We gratefully acknowledge
the strong support from CERN: Rolf-Dieter Heuer, Robert Aymar, and
Luciano Maiani as well as Steve Meyers and Andrzej Siemko. From ESA, we
thank Jean-Jacques Dordain, Simona DiPippo, and Martin Zell for their
support. We are grateful for important discussions with Barry Barish,
Claude Canizares, James Cronin, Jonathan Ellis, Len Fisk, Sheldon
Glashow, Alan Guth, Neal Lane, Steve Olsen, Alvaro de Rujula, Alexander
Rumyantsev, Reinhard Simon, George Smoot, Jian Song, Evgeny Velikhov,
Steven Weinberg, Frank Wilczek, and Cunhao Zhang. Finally, we
acknowledge with appreciation the United States Congress for their
unanimous approval of HR6063 (2008) restoring AMS to the Space Shuttle
manifest and bringing major science to the ISS, and we are grateful for
the support of Joe Barton, Jeff Bingham, Gabrielle Giffords, John Glenn,
Ralph Hall, Kay Bailey Hutchison, Nick Lampson, Bill Nelson, and David
Vitter.; Supported by the Deutsches Zentrum fur Luft- und Raumfahrt,
DLR.; Supported by the National Natural Science Foundation of China.;
Also supported by the Italian Space Agency, ASI.; Also supported by
SEIDI and CPAN.
NR 53
TC 417
Z9 425
U1 29
U2 210
PU AMER PHYSICAL SOC
PI COLLEGE PK
PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA
SN 0031-9007
J9 PHYS REV LETT
JI Phys. Rev. Lett.
PD APR 3
PY 2013
VL 110
IS 14
AR 141102
DI 10.1103/PhysRevLett.110.141102
PG 10
WC Physics, Multidisciplinary
SC Physics
GA 119OJ
UT WOS:000317106800003
PM 25166975
ER
PT J
AU Kelly, BJ
Baker, JG
AF Kelly, Bernard J.
Baker, John G.
TI Decoding mode mixing in black-hole merger ringdown
SO PHYSICAL REVIEW D
LA English
DT Article
ID GRAVITATIONAL-WAVES; SPHERICAL-HARMONICS; GENERAL RELATIVITY; INITIAL
DATA; SPIN; PERTURBATIONS; TIME
AB Optimal extraction of information from gravitational-wave observations of binary black-hole coales-cences requires detailed knowledge of the waveforms. Current approaches for representing waveform information are based on spin-weighted spherical harmonic decomposition. Higher-order harmonic modes carrying a few percent of the total power output near merger can supply information critical to determining intrinsic and extrinsic parameters of the binary. One obstacle to constructing a full multimode template of merger waveforms is the apparently complicated behavior of some of these modes; instead of settling down to a simple quasinormal frequency with decaying amplitude, some vertical bar m vertical bar not equal l modes show periodic bumps characteristic of mode mixing. We analyze the strongest of these modes-the anomalous (3, 2) harmonic mode-measured in a set of binary black-hole merger waveform simulations, and show that to leading order, they are due to a mismatch between the spherical harmonic basis used for extraction in 3D numerical relativity simulations, and the spheroidal harmonics adapted to the perturbation theory of Kerr black holes. Other causes of mode mixing arising from gauge ambiguities and physical properties of the quasinormal ringdown modes are also considered and found to be small for the waveforms studied here. DOI:10.1103/PhysRevD.87.084004
C1 [Kelly, Bernard J.] NASA, Goddard Space Flight Ctr, CRESST, Greenbelt, MD 20771 USA.
[Kelly, Bernard J.; Baker, John G.] NASA, Goddard Space Flight Ctr, Gravitat Astrophys Lab, Greenbelt, MD 20771 USA.
[Kelly, Bernard J.] Univ Maryland Baltimore Cty, Dept Phys, Baltimore, MD 21250 USA.
RP Kelly, BJ (reprint author), NASA, Goddard Space Flight Ctr, CRESST, 8800 Greenbelt Rd, Greenbelt, MD 20771 USA.
OI Kelly, Bernard/0000-0002-3326-4454
FU NASA [09-ATP09-0136]
FX The new numerical evolutions performed for this paper were carried out
on the machine Pleiades at NASA's Ames Research Center. The work was
supported by NASA Grant No. 09-ATP09-0136. The authors would like to
thank Enrico Barausse, Emanuele Berti, Alessandra Buonanno, Rafael
Porto, Luciano Rezzolla, Jeremy Schnittman, and James van Meter for
useful comments.
NR 82
TC 6
Z9 6
U1 0
U2 3
PU AMER PHYSICAL SOC
PI COLLEGE PK
PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA
SN 1550-7998
J9 PHYS REV D
JI Phys. Rev. D
PD APR 2
PY 2013
VL 87
IS 8
AR 084004
DI 10.1103/PhysRevD.87.084004
PG 15
WC Astronomy & Astrophysics; Physics, Particles & Fields
SC Astronomy & Astrophysics; Physics
GA 117LO
UT WOS:000316955100005
ER
PT J
AU Wu, CC
Gopalswamy, N
Lepping, RP
Yashiro, S
AF Wu, Chin-Chun
Gopalswamy, Natchimuthuk
Lepping, Ronld Paul
Yashiro, Seiji
TI Characteristics of Magnetic Clouds and Interplanetary Coronal Mass
Ejections which Cause Intense Geomagnetic Storms
SO TERRESTRIAL ATMOSPHERIC AND OCEANIC SCIENCES
LA English
DT Article
DE Magnetic cloud; Interplanetary coronal mass ejection; Geomagnetic storm;
Solar flare; Corotating interaction region
ID SOLAR; WIND; GEOEFFECTIVENESS; MAXIMUM; EVENTS; CYCLE; CMES
AB We present the results of a statistical data analysis of the geo-effectiveness of non-magnetic-cloud interplanetary coronal mass ejections (ICMEs) and compare them with those of magnetic-cloud (MC) interplanetary coronal mass ejections observed during solar cycle 23. (The term ICME as used here will refer to a non-MC ICME.) The starting point of this investigation is the set of intense geomagnetic storms (Dst(min) <= -100 nT) of solar cycle 23 between 1996 and 2005. We also compare the solar source locations of the ICMEs with those of the MCs. The source locations of the solar disturbances are, on average, closer to the Sun-Earth line for the MCs than for the ICMEs. There is an anomaly for the location of the related solar sources: no event came from the region between the solar equator plane and 10 degrees S (south) of that plane. The primary results are listed as follows. The average duration of these MCs is slightly longer (similar to 7%) than that of ICMEs. The average geomagnetic storm intensity for the MCs is higher than that for the ICMEs and CIRs formed by high-speed streams from coronal holes, especially for the events associated with X class flares. The relevant average magnetic field component, i.e., vertical bar Bz(min) vertical bar, is more intense within the MCs than within the ICMEs. The average solar wind speed is similar for both MCs and ICMEs. Maximum solar wind speed is higher within ICMEs than within MCs. Maximum solar wind proton density is higher for MCs than for ICMEs.
C1 [Wu, Chin-Chun] Naval Res Lab, Washington, DC USA.
[Gopalswamy, Natchimuthuk; Yashiro, Seiji] NASA GSFC, Solar Syst Explorat Div, Solar Phys Lab, Greenbelt, MD USA.
[Lepping, Ronld Paul] NASA GSFC, Heliosphys Sci Div, Greenbelt, MD USA.
[Yashiro, Seiji] Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA.
RP Wu, CC (reprint author), Naval Res Lab, Washington, DC USA.
EM chin-chun.wu@nrl.navy.mil
FU NASA's LWS program [NNH09AM46I]; NRL 6.1 program
FX We thank the Wind SWE and MFI teams and the National Space Science Data
Center at Goddard Space Flight Center for Wind data management and for
providing the Wind solar wind plasma and magnetic field data, and the
team at Kyoto University, Kyoto, Japan for providing the Dst data. This
study is supported partially by NASA's LWS program via grants NNH09AM46I
(CCW and RPL), and NRL 6.1 program (CCW).
NR 31
TC 7
Z9 7
U1 0
U2 4
PU CHINESE GEOSCIENCE UNION
PI TAIPEI
PA PO BOX 23-59, TAIPEI 10764, TAIWAN
SN 1017-0839
J9 TERR ATMOS OCEAN SCI
JI Terr. Atmos. Ocean. Sci.
PD APR
PY 2013
VL 24
IS 2
SI SI
BP 233
EP 241
DI 10.3319/TAO.2012.09.26.03(SEC)
PG 9
WC Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences;
Oceanography
SC Geology; Meteorology & Atmospheric Sciences; Oceanography
GA 292IC
UT WOS:000329894400009
ER
PT J
AU Gao, HY
Wang, ZJ
Huynh, HT
AF Gao, Haiyang
Wang, Z. J.
Huynh, H. T.
TI Differential Formulation of Discontinuous Galerkin and Related Methods
for the Navier-Stokes Equations
SO COMMUNICATIONS IN COMPUTATIONAL PHYSICS
LA English
DT Article
DE Discontinuous Galerkin; lifting collocation penalty; flux
reconstruction; Navier-Stokes equations; correction procedure via
reconstruction; unstructured hybrid grids
ID FINITE-ELEMENT-METHOD; ONE-DIMENSIONAL SYSTEMS; CONSERVATION-LAWS;
UNSTRUCTURED GRIDS; VOLUME METHOD; NUMERICAL-SOLUTION; BASIC
FORMULATION; EULER
AB A new approach to high-order accuracy for the numerical solution of conservation laws introduced by Huynh and extended to simplexes by Wang and Gao is renamed CPR (correction procedure or collocation penalty via reconstruction). The CPR approach employs the differential form of the equation and accounts for the jumps in flux values at the cell boundaries by a correction procedure. In addition to being simple and economical, it unifies several existing methods including discontinuous Galerkin, staggered grid, spectral volume, and spectral difference. To discretize the diffusion terms, we use the BR2 (Bassi and Rebay), interior penalty, compact DG (CDG), and I-continuous approaches. The first three of these approaches, originally derived using the integral formulation, were recast here in the CPR framework, whereas the I-continuous scheme, originally derived for a quadrilateral mesh, was extended to a triangular mesh. Fourier stability and accuracy analyses for these schemes on quadrilateral and triangular meshes are carried out. Finally, results for the Navier-Stokes equations are shown to compare the various schemes as well as to demonstrate the capability of the CPR approach.
C1 [Gao, Haiyang; Wang, Z. J.] Iowa State Univ, Dept Aerosp Engn, Ames, IA 50011 USA.
[Gao, Haiyang; Wang, Z. J.] Iowa State Univ, CFD Ctr, Ames, IA 50011 USA.
[Huynh, H. T.] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA.
RP Gao, HY (reprint author), Iowa State Univ, Dept Aerosp Engn, 2271 Howe Hall Ames, Ames, IA 50011 USA.
EM hgao@iastate.edu; zjw@iastate.edu; hung.t.huynh@nasa.gov
RI Wang, Z.J./A-9628-2010
OI Wang, Z.J./0000-0002-6203-6303
FU AFOSR [FA9550-06-1-0146]; NASA's Fundamental Aeronautics Program
FX The first two authors were funded by AFOSR grant FA9550-06-1-0146. The
third author is supported by NASA's Fundamental Aeronautics Program. The
views and conclusions contained herein are those of the authors and
should not be interpreted as necessarily representing the official
policies or endorsements, either expressed or implied, of AFOSR, NASA or
the U.S. Government.
NR 29
TC 8
Z9 8
U1 0
U2 7
PU GLOBAL SCIENCE PRESS
PI WANCHAI
PA ROOM 3208, CENTRAL PLAZA, 18 HARBOUR RD, WANCHAI, HONG KONG 00000,
PEOPLES R CHINA
SN 1815-2406
J9 COMMUN COMPUT PHYS
JI Commun. Comput. Phys.
PD APR
PY 2013
VL 13
IS 4
BP 1013
EP 1044
DI 10.4208/cicp.020611.090312a
PG 32
WC Physics, Mathematical
SC Physics
GA 186SN
UT WOS:000322065200004
ER
PT J
AU Schwalm, CR
Huntinzger, DN
Michalak, AM
Fisher, JB
Kimball, JS
Mueller, B
Zhang, K
Zhang, YQ
AF Schwalm, Christopher R.
Huntinzger, Deborah N.
Michalak, Anna M.
Fisher, Joshua B.
Kimball, John S.
Mueller, Brigitte
Zhang, Ke
Zhang, Yongqiang
TI Sensitivity of inferred climate model skill to evaluation decisions: a
case study using CMIP5 evapotranspiration
SO ENVIRONMENTAL RESEARCH LETTERS
LA English
DT Article
DE climate models; model validation; evapotranspiration; CMIP5
ID LAND-SURFACE MODELS; CARBON; BENCHMARK; WATER; AVHRR
AB Confrontation of climate models with observationally-based reference datasets is widespread and integral to model development. These comparisons yield skill metrics quantifying the mismatch between simulated and reference values and also involve analyst choices, or meta-parameters, in structuring the analysis. Here, we systematically vary five such meta-parameters (reference dataset, spatial resolution, regridding approach, land mask, and time period) in evaluating evapotranspiration (ET) from eight CMIP5 models in a factorial design that yields 68 700 intercomparisons. The results show that while model-data comparisons can provide some feedback on overall model performance, model ranks are ambiguous and inferred model skill and rank are highly sensitive to the choice of meta-parameters for all models. This suggests that model skill and rank are best represented probabilistically rather than as scalar values. For this case study, the choice of reference dataset is found to have a dominant influence on inferred model skill, even larger than the choice of model itself. This is primarily due to large differences between reference datasets, indicating that further work in developing a community-accepted standard ET reference dataset is crucial in order to decrease ambiguity in model skill.
C1 [Schwalm, Christopher R.; Huntinzger, Deborah N.] No Arizona Univ, Sch Earth Sci & Environm Sustainabil, Flagstaff, AZ 86011 USA.
[Huntinzger, Deborah N.] No Arizona Univ, Dept Civil Engn Construct Management & Environm E, Flagstaff, AZ 86011 USA.
[Michalak, Anna M.] Carnegie Inst Sci, Dept Global Ecol, Stanford, CA 94305 USA.
[Fisher, Joshua B.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Kimball, John S.] Univ Montana, Flathead Lake Biol Stn, Div Biol Sci, Polson, MT 59860 USA.
[Mueller, Brigitte] ETH, Inst Atmospher & Climate Sci, CH-8092 Zurich, Switzerland.
[Zhang, Ke] Harvard Univ, Dept Organism & Evolutionary Biol, Cambridge, MA 02138 USA.
[Zhang, Yongqiang] CSIRO Land & Water, Canberra, ACT, Australia.
RP Schwalm, CR (reprint author), No Arizona Univ, Sch Earth Sci & Environm Sustainabil, Flagstaff, AZ 86011 USA.
EM christopher.schwalm@nau.edu
RI Zhang, Yongqiang/C-5708-2008; Mueller, Brigitte/E-2594-2011; Zhang,
Ke/B-3227-2012;
OI Zhang, Yongqiang/0000-0002-3562-2323; Mueller,
Brigitte/0000-0003-1876-4722; Zhang, Ke/0000-0001-5288-9372; Fisher,
Joshua/0000-0003-4734-9085
FU National Aeronautics and Space Administration (NASA) [NNX10AG01A,
NNX12AK12G]
FX We acknowledge the World Climate Research Programme's Working Group on
Coupled Modelling, which is responsible for CMIP, and we thank the
climate modeling groups for producing and making available their model
output. For CMIP the US Department of Energy's Program for Climate Model
Diagnosis and Intercomparison provides coordinating support and led
development of software infrastructure in partnership with the Global
Organization for Earth System Science Portals. CRS, DNH, and AMM were
supported by the National Aeronautics and Space Administration (NASA)
under Grant No. NNX10AG01A 'The NACP Multi-Scale Synthesis and
Terrestrial Model Intercomparison Project (MsTMIP)'. CRS was also
supported by NASA Grant No. NNX12AK12G. JBF contributed to this paper at
the Jet Propulsion Laboratory, California Institute of Technology under
a contract with NASA.
NR 25
TC 16
Z9 16
U1 2
U2 20
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 1748-9326
J9 ENVIRON RES LETT
JI Environ. Res. Lett.
PD APR-JUN
PY 2013
VL 8
IS 2
AR 024028
DI 10.1088/1748-9326/8/2/024028
PG 9
WC Environmental Sciences; Meteorology & Atmospheric Sciences
SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences
GA 178DU
UT WOS:000321425100032
ER
PT J
AU Murthy, R
Stephanou, HE
Popa, DO
AF Murthy, Rakesh
Stephanou, Harry E.
Popa, Dan O.
TI AFAM: An Articulated Four Axes Microrobot for Nanoscale Applications
SO IEEE TRANSACTIONS ON AUTOMATION SCIENCE AND ENGINEERING
LA English
DT Article
DE Microassembly; microelectromechanical systems (MEMS); microrobot
ID ROBOTICS
AB This paper presents a microassembled robot called the Articulated Four Axes Microrobot (AFAM). Target application areas include micro and nano part manipulation and probing. The robot consists of a cantilever actuated along four axes: in-place X, Y and Y AW; out-of-plane pitch. The microrobot size spans a total volume of 3 mm x 1.5 mm x 1 mm (XYZ), and operates within a workspace envelope of 50 mu m x 50 mu m x 75 mu m (XYZ). This is by far the largest operating envelope of any micropositioner with nonplanar dexterity. As a result it can be classified as a new type of three-dimensional microrobot and a candidate for miniaturizing top-down assembly systems to dimensions under 1 cm(3). A key feature in this design is a cable-like microwire that transforms in-plane actuator displacement into out-of-plane pitch and yaw motion (via flexure joints). Finite-element analysis simulation followed by microfabrication and assembly processes developed to prototype the designs are described. The microrobot is designed to carry an AFM tip as the end effector and accomplish nanoindentation on a polymer surface. The tip attachment technique and nanoindentation experiments have also been described in this paper. Open loop precision has been characterized using a laser interferometer which measured an average resolution of 50 nm along XYZ, repeatability of 100 nm and accuracy of 500 nm. Experiments to determine microrobot reliability are also presented.
Note to Practitioners-Micro/nanosystems research and development incorporates a large variety of tools and processes in order to accomplish high precision fabrication, assembly, testing and characterization. A very common component in these tools is high precision positioning units (robots) that are a combination of linear and rotary subunits (stages). Their role is to position micro or nanocomponents, substrates or wafers in an accurately and repeatable manner. Current state-of-art positioners typically span few inches to many feet in size. Although they are able to deliver the required precision, range of motion, and dexterity, their size inhibits the merger of multiple units under a common platform leading to throughput limitations. This paper presents an attempt to develop a new class of miniaturized robots that span no more than a few cubic millimeters in size, while delivering a subset of the capabilities as traditional macroscale equivalents. The tradeoffs between robot size, stiffness, range of motion, dexterity, and precision is taken to a new level where the robots are no more than two or three orders of magnitude larger than the smallest parts being manufactured.
C1 [Murthy, Rakesh] Jet Prop Lab, Instrument Elect & Sensors Div, Nano & Micro Syst Grp, Passadena, CA 91109 USA.
[Stephanou, Harry E.; Popa, Dan O.] Univ Texas Arlington, Arlington, TX 76011 USA.
RP Murthy, R (reprint author), Jet Prop Lab, Instrument Elect & Sensors Div, Nano & Micro Syst Grp, Passadena, CA 91109 USA.
EM rakesh.murthy@jpl.nasa.gov; popa@arri.uta.edu
FU Office of Naval Research
FX This work was supported by the Office of Naval Research and carried out
at Automation and Robotics Research Institute, the University of Texas
at Arlington.
NR 21
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U1 5
U2 24
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 1545-5955
J9 IEEE T AUTOM SCI ENG
JI IEEE Trans. Autom. Sci. Eng.
PD APR
PY 2013
VL 10
IS 2
BP 276
EP 284
DI 10.1109/TASE.2012.2217740
PG 9
WC Automation & Control Systems
SC Automation & Control Systems
GA 172IF
UT WOS:000320994500006
ER
PT J
AU Ostrikov, K
Neyts, EC
Meyyappan, M
AF Ostrikov, K.
Neyts, E. C.
Meyyappan, M.
TI Plasma nanoscience: from nano-solids in plasmas to nano-plasmas in
solids
SO ADVANCES IN PHYSICS
LA English
DT Review
DE nanoscale solid systems; self-organization; plasma-specific effects;
structural and functional properties; nano-plasmas
ID CHEMICAL-VAPOR-DEPOSITION; WALLED CARBON NANOTUBES; LOW-TEMPERATURE
GROWTH; INDUCTIVELY-COUPLED PLASMA; SURFACE LOSS PROBABILITIES;
METAL-OXIDE NANOWIRES; DIAMOND-LIKE CARBON; WARM DENSE MATTER; GRAPHENE
NANORIBBONS; SOLAR-CELLS
AB The unique plasma-specific features and physical phenomena in the organization of nanoscale soild-state systems in a broad range of elemental composition, structure, and dimensionality are critically reviewed. These effects lead to the possibility to localize and control energy and matter at nanoscales and to produce self-organized nano-solids with highly unusual and superior properties. A unifying conceptual framework based on the control of production, transport, and self-organization of precursor species is introduced and a variety of plasma-specific non-equilibrium and kinetics-driven phenomena across the many temporal and spatial scales is explained. When the plasma is localized to micrometer and nanometer dimensions, new emergent phenomena arise. The examples range from semiconducting quantum dots and nanowires, chirality control of single-walled carbon nanotubes, ultra-fine manipulation of graphenes, nano-diamond, and organic matter to nano-plasma effects and nano-plasmas of different states of matter.
C1 [Ostrikov, K.] CSIRO Mat Sci & Engn, Lindfield, NSW 2070, Australia.
[Neyts, E. C.] Univ Antwerp, Dept Chem, Res Grp PLASMANT, B-2610 Antwerp, Belgium.
[Meyyappan, M.] NASA Ames Res Ctr, Moffett Field, CA 94035 USA.
RP Ostrikov, K (reprint author), CSIRO Mat Sci & Engn, POB 218, Lindfield, NSW 2070, Australia.
EM kostya.ostrikov@csiro.au
RI Neyts, Erik/H-4198-2012;
OI Neyts, Erik/0000-0002-3360-3196; Ostrikov, Kostya
(Ken)/0000-0001-8672-9297
FU Australian Research Council; CSIRO's Science Leadership Program; ARC
Future Fellowship
FX We sincerely thank many our colleagues for fruitful collaborations,
discussions, and critical comments with apologies of not being able to
mention by name due to limited space. We also thank all authors of
original figures for the permissions to reproduce. This work was
partially supported by the Australian Research Council and CSIRO's
Science Leadership Program. K. O. is grateful to the University of
Sydney (Australia) and Nanyang Technological University (Singapore) as
Host Organizations for his ARC Future Fellowship as well as Huazhong
University of Science and Technology (China), the University of
Technology Sydney (Australia), and the University of Wollongong
(Australia) for the visiting, adjunct, and honorary professor support.
We are particularly thankful to the anonymous referee for the insightful
discussion of states of matter and phase transitions at nanoscales. We
also thank every person who has ever contributed to the relevant areas
and apologize for not being able to include all these results, although
would certainly do that if that were physically possible.
NR 393
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U2 284
PU TAYLOR & FRANCIS LTD
PI ABINGDON
PA 4 PARK SQUARE, MILTON PARK, ABINGDON OX14 4RN, OXON, ENGLAND
SN 0001-8732
EI 1460-6976
J9 ADV PHYS
JI Adv. Phys.
PD APR 1
PY 2013
VL 62
IS 2
BP 113
EP 224
DI 10.1080/00018732.2013.808047
PG 112
WC Physics, Condensed Matter
SC Physics
GA 171GQ
UT WOS:000320913600001
ER
PT J
AU Stoner, AW
Copeman, LA
Ottmar, ML
AF Stoner, Allan W.
Copeman, Louise A.
Ottmar, Michele L.
TI Molting, growth, and energetics of newly-settled blue king crab: Effects
of temperature and comparisons with red king crab
SO JOURNAL OF EXPERIMENTAL MARINE BIOLOGY AND ECOLOGY
LA English
DT Article
DE Bioenergetics; Culture; Fatty acid; Growth; Lipid; Paralithodes
platypus; Temperature
ID PARALITHODES-PLATYPUS BRANDT; MOLECULAR-SPECIES COMPOSITION; FATTY-ACID
COMPOSITION; BERING-SEA; CLIMATE-CHANGE; LIPID-COMPOSITION;
EMBRYONIC-DEVELOPMENT; CALLINECTES-SAPIDUS; LITHODES-SANTOLLA; STOCK
ENHANCEMENT
AB Populations of blue king crab (BKC) (Paralithodes platypus Brandt, 1850) have declined in Alaskan waters over recent decades, and substantial effort is being made to rehabilitate the once important fishery with releases of hatchery-reared juveniles. However, little is known about the species' first year of post-settlement life. This study was conducted to evaluate how temperature mediates growth and energy allocation beginning with the first benthic instar (stage C1). Juvenile BKC were reared in four temperatures (1.5 to 12 degrees C) for a period of 60 days in low-density populations (150 crabs m(-2)) and 120 days in individual cultures. Growth rate increased rapidly up to 8 degrees C, and then leveled off. At 60 days, most of the crabs in 1.5 degrees C remained at stage C1, most in 4.5 degrees C were C2, and most in 8 degrees C were C3, while those in 12 degrees C were highly variable and ranged from C2 to C5. Growth records for individuals revealed an inverse exponential relationship between water temperature and intermolt period (up to 8 degrees C). A small decrease in molt increment at 12 degrees C resulted in crabs 6% smaller than those at 8 degrees C. Total lipid content increased with temperature in C2 BKC, but the response was variable and not significant in later stages. The proportion of storage class lipids (triacylglycerols) increased with an increase in temperature and polar lipids decreased. Concentrations of essential fatty acids were relatively constant over all temperature treatments, indicating that temperature and growth rate did not affect the biochemical condition of juvenile BKC. Survival rates of BKC (>95%) were similar across temperatures and were much higher than rates observed for red king crab (RKC) (Paralithodes camchaticus Tilesius 1815) (65-72%) in identical experiments. Growth rates of the two species were nearly identical up to 8 degrees C, but RKC grew faster than BKC at temperatures greater than 8 degrees C, with more molts resulting in larger individuals. Fatty acid (FA) signatures supported the lipid class data and showed that BKC had higher proportions of FA associated with energy storage while RKC had higher proportions of polyunsaturated FAs associated with membranes. These results indicate that BKC are the hardier species, and it shows little sign of cannibalism in culture (unlike RKC), but RKC grow faster at high temperature and are less vulnerable to warming climate. These data help to model temperature-dependent recruitment processes in the field and assist in the design of diets and hatchery conditions for production of seed stocks intended for field release. Published by Elsevier B.V.
C1 [Stoner, Allan W.; Ottmar, Michele L.] NOAA, Fisheries Behav Ecol Program, Alaska Fisheries Sci Ctr, Natl Marine Fisheries Serv, Newport, OR 97365 USA.
[Copeman, Louise A.] Oregon State Univ, Hatfield Marine Sci Ctr, Cooperat Inst Marine Resources Studies, Newport, OR 97365 USA.
RP Stoner, AW (reprint author), NOAA, Fisheries Behav Ecol Program, Alaska Fisheries Sci Ctr, Natl Marine Fisheries Serv, 2030 S,Marine Sci Dr, Newport, OR 97365 USA.
EM allan.stoner@gmail.com
FU NOAA Aquaculture Program; Alaska Sea Grant College Program
FX This study was conducted as part of the AKCRRAB Program (Alaska King
Crab Research, Rehabilitation, and Biology) funded in part by the NOAA
Aquaculture Program and the Alaska Sea Grant College Program. Crabs were
provided by the Alutiiq Pride Shellfish Hatchery, Seward, AK, with
special thanks to B. Daly and J. Swingle who cultured the larvae for
this experiment. Assistance with apparatus and maintenance of the
cultures in Newport was provided by S. Haines, P. Iseri, and C. Danley.
A. Sremba assisted with the lipid and fatty acid analyses. Thanks also
to Drs. B. MacFarlane and S. Sogard for the long-term loan of the
Iatroscan TLC-FID system for lipid class analyses. B. Daly and T. Hurst
provided helpful reviews for the manuscript. [SS]
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PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0022-0981
EI 1879-1697
J9 J EXP MAR BIOL ECOL
JI J. Exp. Mar. Biol. Ecol.
PD APR
PY 2013
VL 442
BP 10
EP 21
DI 10.1016/j.jembe.2013.02.002
PG 12
WC Ecology; Marine & Freshwater Biology
SC Environmental Sciences & Ecology; Marine & Freshwater Biology
GA 164QW
UT WOS:000320425600002
ER
PT J
AU Frey, A
Dutton, PH
Balazs, GH
AF Frey, Amy
Dutton, Peter H.
Balazs, George H.
TI Insights on the demography of cryptic nesting by green turtles (Chelonia
mydas) in the main Hawaiian Islands from genetic relatedness analysis
SO JOURNAL OF EXPERIMENTAL MARINE BIOLOGY AND ECOLOGY
LA English
DT Article
DE Chelonia mydas; Founder event; Kinship; Microsatellite; Relatedness; Sea
turtles
ID MULTILOCUS GENOTYPE DATA; NATURAL-POPULATIONS; PARENTAGE ANALYSIS;
SIBSHIP INFERENCE; MARINE TURTLES; CONSERVATION; RECOVERY;
RECONSTRUCTION; MARKERS; ERRORS
AB Within the Hawaiian archipelago, green turtle nesting has occurred almost exclusively in the northwestern Hawaiian Islands, mainly at French Frigate Shoals (FFS), however an increase in occasional nesting has recently been observed on the main Hawaiian Islands (MHI). Due to logistical constraints, monitoring the nesting activity on the MHI has been limited to nest documentation. Without systematic tagging of the nesting females it is not clear how many are nesting here. We used mitochondrial (mt) DNA sequencing combined with nuclear (n) DNA analysis based on 14 microsatellite markers to infer the number of individual nesters. Genotypes were determined for 181 dead embryos and hatchlings salvaged from 71 nests laid on Maui, Molokai, Kauai, Lanai, and Oahu, along with those of 81 nesting females that were sampled on FFS. MtDNA results showed that 58% of the MHI clutches were laid by females with a relatively rare haplotype only reported in 16% of the FFS nesting population. Nuclear DNA results showed that nesting in the MHI might be attributed to a relatively small number of females that appear to be related to each other. We were able to reconstruct genotypes for nesting females from hatchling profiles and we estimate that 15 different females were responsible for clutches laid on the MHI. Taken together, the mtDNA and nDNA results suggest that the nesting population at the MHI may be the result of a few founders that originated from the FFS breeding population, possibly facilitated by captive rearing and release of FFS juveniles locally from Oahu. We suggest that this regional range expansion may buffer against the loss of current nesting sites at FFS due to sea level rise. Our results demonstrate the potential for genetic tools to be incorporated into population assessment, particularly in areas where access to reproductive females is difficult and population size is unknown. Published by Elsevier B.V.
C1 [Frey, Amy; Dutton, Peter H.] NOAA, Natl Marine Fisheries Serv, SW Fisheries Sci Ctr, Protected Resources Div, La Jolla, CA 92037 USA.
[Balazs, George H.] NOAA, Natl Marine Fisheries Serv, Pacific Isl Fisheries Sci Ctr, Honolulu, HI 96822 USA.
RP Frey, A (reprint author), NOAA, Natl Marine Fisheries Serv, SW Fisheries Sci Ctr, Protected Resources Div, 8901 La Jolla Shores Dr, La Jolla, CA 92037 USA.
EM Amy.Frey@noaa.gov
FU NOAA-National Marine Fisheries Service
FX Thanks to the Molokai Turtle Trackers, Nature Conservancy community
volunteers who monitored nesting tracks and nests. Samples from the
Hawaiian Islands National Wildlife Refuge were overseen by the USFWS,
Department of the Interior. We'd like to thank Stacy Hargrove, Kelly
Stewart, Erin LaCasella, Amy Jue, Gabriela Serra-Valente, Amanda Bowman,
Michael Jensen, Suzanne Roden, Brad McDonald and Robin LeRoux for their
help at the lab and with the data. This study was funded by
NOAA-National Marine Fisheries Service. [RH]
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PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0022-0981
J9 J EXP MAR BIOL ECOL
JI J. Exp. Mar. Biol. Ecol.
PD APR
PY 2013
VL 442
BP 80
EP 87
DI 10.1016/j.jembe.2013.01.030
PG 8
WC Ecology; Marine & Freshwater Biology
SC Environmental Sciences & Ecology; Marine & Freshwater Biology
GA 164QW
UT WOS:000320425600010
ER
PT J
AU Maselko, J
Bishop, G
Murphy, P
AF Maselko, Jacek
Bishop, Gretchen
Murphy, Peter
TI Ghost Fishing in the Southeast Alaska Commercial Dungeness Crab Fishery
SO NORTH AMERICAN JOURNAL OF FISHERIES MANAGEMENT
LA English
DT Article
ID CANCER-MAGISTER; TRAP; ESTUARY; POTS
AB Entrapment of crabs by derelict crab pots (also known as ghost fishing) can be a significant consequence of commercial fishing. The prevalence of lost commercial pots and ghost-fishing entrapments was estimated for the commercial Dungeness crab Cancer magister fishery in southeastern Alaska during the 2009 and 2010 summer closures of the commercial season (16 August through 30 September). Teams of divers retrieved a random subsample of the derelict crab pots located using side-scan sonar. Altogether, we retrieved 123 derelict crab pots containing 215 entrapped Dungeness crabs. The densities of derelict crab pots varied from 1.5 to 10.1/km(2), while the densities of entrapped Dungeness crabs ranged from 0 to 54.5/km(2), depending on the area surveyed. Derelict crab pots were discovered to effectively ghost-fish for at least 7years, indicating that there are long-term cumulative impacts on Dungeness crab populations. The number of derelict crab pots and entrapped Dungeness crabs at each of the surveyed areas was highly correlated with the number of fishermen, the number of pot lifts, and annual harvest in numbers, allowing for extrapolation to a regionwide estimate of crab entrapment and derelict crab pot abundance. Overall, our findings show instantaneous entrapment of less than 1% of the commercial crab harvest with a cumulative annual loss of less than 3% of the regional commercial crab harvest. We challenge the efficacy of the biodegradable escape mechanism currently employed in commercial Dungeness crab pots in southeastern Alaska and present alternatives which may require further in situ or laboratory verification of their effectiveness.
C1 [Maselko, Jacek] Alaska Fisheries Sci Ctr, Natl Marine Fisheries Serv, Auke Bay Labs, Juneau, AK 99801 USA.
[Bishop, Gretchen] Alaska Dept Fish & Game, Div Commercial Fisheries, Juneau, AK 99811 USA.
[Murphy, Peter] NOAA, Marine Debris Program, Off Response & Restorat, Seattle, WA 98115 USA.
RP Maselko, J (reprint author), Alaska Fisheries Sci Ctr, Natl Marine Fisheries Serv, Auke Bay Labs, 17109 Point Lena Loop Rd, Juneau, AK 99801 USA.
EM jacek.maselko@noaa.gov
FU NOAA Marine Debris Division
FX This study was funded by the NOAA Marine Debris Division. Special thanks
to Eric Brown, Andrew Eller, and Haley Poole for help with field work
and data processing and to the divers: Manuel Cruz, Peter Fischel, David
Francksen, Bill Heard, Justin Keese, Pat Malecha, Jennifer Mondragon,
Matthew Nardi, Kalei Shotwell, Elizabeth Siddon, Bob Stone, Ryan Wattam,
Brad Weinlaeder, and Alex Wertheimer. We also thank the reviewers for
their invaluable contribution. Reference to trade names does not imply
endorsement by the U.S. Government. The findings and conclusions in this
report are those of the author(s) and do not necessarily represent the
views of the funding agency.
NR 29
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U1 1
U2 14
PU TAYLOR & FRANCIS INC
PI PHILADELPHIA
PA 325 CHESTNUT ST, SUITE 800, PHILADELPHIA, PA 19106 USA
SN 0275-5947
J9 N AM J FISH MANAGE
JI North Am. J. Fish Manage.
PD APR 1
PY 2013
VL 33
IS 2
BP 422
EP 431
DI 10.1080/02755947.2013.763875
PG 10
WC Fisheries
SC Fisheries
GA 167PD
UT WOS:000320643000020
ER
PT J
AU Liston, DB
Krukowski, AE
Stone, LS
AF Liston, Dorion B.
Krukowski, Anton E.
Stone, Leland S.
TI Saccade detection during smooth tracking
SO DISPLAYS
LA English
DT Article
DE Eye movements; Saccades; Smooth pursuit; Fixation
ID PURSUIT EYE-MOVEMENTS; VESTIBULO-OCULAR REFLEX; MONKEY; PERCEPTION;
FREQUENCIES; EXPANSION; MECHANICS; FIXATION; LATENCY; SEARCH
AB Saccade detection in an eye-movement trace provides a starting point for analyses ranging from the investigation of low-level oculomotor mechanisms to high-level cognitive processes. When the eye tracks the motion of the object of current interest (smooth pursuit), of the visual background (OKN), or of the resultant visual motion from a head movement (tVOR, rVOR), the smooth tracking movement is generally intermixed with rapid-phase saccadic eye movements, which must be excised to analyze the smooth components of tracking behavior properly. We describe a simple method to detect saccades on a background trace of variable velocity, compare our saccade-detection algorithm with the performance of an expert human observer, and present an ideal-observer analysis to benchmark its detection performance. (c) 2012 Elsevier B.V. All rights reserved.
C1 [Liston, Dorion B.; Krukowski, Anton E.; Stone, Leland S.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Liston, Dorion B.; Krukowski, Anton E.] San Jose State Univ, San Jose, CA 95192 USA.
RP Liston, DB (reprint author), NASA, Ames Res Ctr, Mail Stop 262-2, Moffett Field, CA 94035 USA.
EM dorion.b.liston@nasa.gov
FU NSF's Program in Perception, Action and Cognition [NSF 0924841];
National Aeronautics and Space Administration (National Space Biomedical
Research Institute Grant) [SA2002]
FX This work was supported by NSF's Program in Perception, Action and
Cognition (NSF 0924841 to DL) and the National Aeronautics and Space
Administration (National Space Biomedical Research Institute Grant
SA2002 to LS). We thank Chad Netzer and Rami Ersheid for technical
assistance and Brent Beutter for helpful suggestions on this manuscript.
NR 40
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PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0141-9382
J9 DISPLAYS
JI Displays
PD APR
PY 2013
VL 34
IS 2
BP 171
EP 176
DI 10.1016/j.displa.2012.10.002
PG 6
WC Computer Science, Hardware & Architecture; Engineering, Electrical &
Electronic; Instruments & Instrumentation; Optics
SC Computer Science; Engineering; Instruments & Instrumentation; Optics
GA 163PR
UT WOS:000320349900014
ER
PT J
AU Scalo, C
Boegman, L
Piomelli, U
AF Scalo, C.
Boegman, L.
Piomelli, U.
TI Large-eddy simulation and low-order modeling of sediment-oxygen uptake
in a transitional oscillatory flow
SO JOURNAL OF GEOPHYSICAL RESEARCH-OCEANS
LA English
DT Article
DE sediment oxygen uptake; seiche dynamics; high Schmidt number; mass
transfer; transitional flow; oscillating boundary layer
ID BOUNDARIES INTERFACIAL FLUX; LAKE-ERIE; BOTTOM-BOUNDARY; WATER
INTERFACE; HEAT-TRANSFER; TURBULENCE; NUMBERS; LAYERS; BED;
PHYTOPLANKTON
AB We have tested a dissolved oxygen (DO) transport model based on large-eddy simulation (LES) of a transitional oscillatory flow observed in the bottom boundary layer of Lake Alpnach, Switzerland. The transition from a quasi-laminar to a fully turbulent state makes this flow difficult to study with a Reynolds-averaged Navier-Stokes equation (RANSE) model. By resolving the full range of governing transport processes, LES provides a reliable prediction of the sediment-oxygen uptake (SOU). The model biogeochemical and flow parameters have been calibrated against DO and velocity measurements from published in situ data at the earliest phase available in the cycle. The fully developed flow thus obtained is used as an initial condition for the imposed oscillatory forcing. Numerical predictions show that transport in the outer layer is in equilibrium with the main current throughout most of the cycle and that nonequilibrium effects are limited to the diffusive sublayer response to the external forcing. During flow deceleration, the concentration boundary layer slowly expands as turbulence decays; later, during re-transition, mixing is restored by rapid and intense turbulent production events enhancing the SOU with a well-defined time lag. An algebraic model for the SOU is proposed for eventual inclusion in RANSE biogeochemical management-type models developed based on parameterizations used in turbulent mass transfer and with the support of published numerical data and the present simulation. The only input parameters required are the sediment oxidation rate, bulk temperature and DO concentration, and friction velocity.
C1 [Scalo, C.; Piomelli, U.] Queens Univ, Dept Mech & Mat Engn, Kingston, ON, Canada.
[Boegman, L.] Queens Univ, Dept Civil Engn, Kingston, ON K7L 3N6, Canada.
RP Scalo, C (reprint author), Stanford Univ, NASA, Ctr Turbulence Res, Bldg 500, Stanford, CA 94305 USA.
EM cscalo.ca@gmail.com
FU Natural Science and Engineering Research Council of Canada; Canada
Research Chair program
FX We acknowledge the financial support of the Natural Science and
Engineering Research Council of Canada under the Discovery Grant Program
and the Canada Research Chair program. The authors also thank the High
Performance Computing Virtual Laboratory (HPCVL), Queen's University
site, for the computational support. The authors thank Damien Bouffard
for the fruitful discussions on the flow physics, field-scale
measurements, on the parametrization of the sediment-oxygen uptake and
for providing us with his field data.
NR 49
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PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-9275
J9 J GEOPHYS RES-OCEANS
JI J. Geophys. Res.-Oceans
PD APR
PY 2013
VL 118
IS 4
BP 1926
EP 1939
DI 10.1002/jgrc.20113
PG 14
WC Oceanography
SC Oceanography
GA 163GN
UT WOS:000320324100020
ER
PT J
AU Qu, TD
Gao, S
Fukumori, I
AF Qu, Tangdong
Gao, Shan
Fukumori, Ichiro
TI Formation of salinity maximum water and its contribution to the
overturning circulation in the North Atlantic as revealed by a global
general circulation model
SO JOURNAL OF GEOPHYSICAL RESEARCH-OCEANS
LA English
DT Article
DE salinity maximum; formation; overturning circulation; North Atlantic
ID SEA-SURFACE SALINITY; TROPICAL ATLANTIC; OCEAN; PATHWAYS; PACIFIC;
TRENDS; DEEP; CLIMATOLOGY; VARIABILITY; VENTILATION
AB The formation of salinity maximum water in the North Atlantic is investigated using a simulated passive tracer and its adjoint. The results reveal that most salinity maximum water in the North Atlantic comes from the northwestern part of the subtropical gyre, and direct contribution from the evaporation-precipitation maximum region via the surface Ekman current is minor. Water originating from the evaporation-precipitation maximum region has to recirculate in the subtropical gyre before entering the sea surface salinity maximum region from the northwest. Once subducted, some portion (similar to 10%) of the salinity maximum water enters the equatorial region in the shallow subtropical cell, but most (similar to 70%) of it appears to turn northward to join the North Atlantic Deep Water. The latter pathway involves a three-dimensional circulation. When the warm, fresh surface water flows northward along the western boundary, it turns eastward in the northern subtropical gyre. As a result of the large excess of evaporation over precipitation, this water gradually gains its salinity on the route, until it reaches the sea surface salinity maximum region in the central subtropical gyre. From there, the salinity maximum water is subducted and flows back to the western boundary in the depth range of the thermocline. With its high-salinity nature, a major portion of this water penetrates into the subpolar region and directly contributes to the deep thermohaline circulation.
C1 [Qu, Tangdong; Gao, Shan] Univ Hawaii Manoa, Int Pacific Res Ctr, SOEST, Honolulu, HI 96822 USA.
[Fukumori, Ichiro] CALTECH, Jet Prop Lab, Pasadena, CA USA.
RP Qu, TD (reprint author), Univ Hawaii Manoa, Int Pacific Res Ctr, SOEST, 1680 East West Rd, Honolulu, HI 96822 USA.
EM tangdong@hawaii.edu
RI Gao, Shan/H-7959-2013
OI Gao, Shan/0000-0003-4510-5028
FU NASA
FX This research was supported by NASA as part of the Aquarius Science Team
investigation. The OAFlux evaporation climatology was downloaded at
ftp://ftp.whoi.edu/pub/science/oaflux/data_v3 and the GPCP precipitation
climatology at ftp://rsd.gsfc.nasa.gov/pub/gpcp-v2.2cl, both through the
Asian Pacific Data Research Center at http://apdrc.soest.hawaii.edu. The
authors thank the three anonymous reviewers for their thoughtful
comments and constructive suggestions on an earlier version of the
manuscript. School of Ocean and Earth Science and Technology
contribution number 8885, and International Pacific Research Center
contribution number IPRC-953.
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PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-9275
J9 J GEOPHYS RES-OCEANS
JI J. Geophys. Res.-Oceans
PD APR
PY 2013
VL 118
IS 4
BP 1982
EP 1994
DI 10.1002/jgrc.20152
PG 13
WC Oceanography
SC Oceanography
GA 163GN
UT WOS:000320324100024
ER
PT J
AU Moon, JH
Song, YT
AF Moon, Jae-Hong
Song, Y. Tony
TI Sea level and heat content changes in the western North Pacific
SO JOURNAL OF GEOPHYSICAL RESEARCH-OCEANS
LA English
DT Article
DE Sea level rise; oceanic heat content; non-Boussinesq OGCM; ocean mass;
western North Pacific
ID SOUTH CHINA SEA; TROPICAL PACIFIC; SATELLITE ALTIMETRY; OCEAN;
VARIABILITY; TRENDS; BUDGET; RISE; SURFACE; SYSTEM
AB Altimetry-observed sea level rise (SLR) over the western North Pacific (WNP), including the South China Sea, Yellow Sea, East China Sea, and East/Japan Sea, has a rate of 5 mm/year over 1993-2010, which is about 1.5 times the rate of the global mean. Here we have examined sea level changes and related ocean heat content (OHC) in the WNP by comparing results from a non-Boussinesq ocean general circulation model (mass-conserved) with data sets from altimeters, the Gravity Recovery and Climate Experiment (GRACE), and in situ profiles. Our model reproduces the altimetry regional trends as well as their seasonal/interannual variations. Adding a GRACE-estimated mass to the model result further explains the altimetry SLR in a way that mass-induced effect contributes more in the midlatitudes than in the tropical WNP over the GRACE period. In addition, interannual variability and linear trend of regional sea levels are explained mainly by changes in the OHC due to heat convergence and divergence by ocean circulations, while seasonal variability is caused mainly by surface air-sea fluxes. To understand the underline physics, a comparative experiment was carried out, showing that the recent strengthening trends of SLR and OHC in the tropical regions are significantly attributed to the heat and water mass redistribution in the upper ocean caused by the intensified easterly trade wind over the past two decades.
C1 [Moon, Jae-Hong; Song, Y. Tony] CALTECH, Jet Prop Lab, Pasadena, CA 91106 USA.
RP Moon, JH (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91106 USA.
EM Jae-Hong.Moon@jpl.nasa.gov
NR 42
TC 8
Z9 9
U1 1
U2 24
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-9275
EI 2169-9291
J9 J GEOPHYS RES-OCEANS
JI J. Geophys. Res.-Oceans
PD APR
PY 2013
VL 118
IS 4
BP 2014
EP 2022
DI 10.1002/jgrc.20096
PG 9
WC Oceanography
SC Oceanography
GA 163GN
UT WOS:000320324100026
ER
PT J
AU Kidd, C
Srinivasan, J
Roca, R
AF Kidd, Chris
Srinivasan, J.
Roca, Remy
TI The Megha-Tropiques mission: day 1 algorithms
SO QUARTERLY JOURNAL OF THE ROYAL METEOROLOGICAL SOCIETY
LA English
DT Editorial Material
C1 [Kidd, Chris] Univ Maryland, ESSIC, NASA GSFC, Greenbelt, MD USA.
[Srinivasan, J.] Indian Inst Sci, Ctr Atmospher & Ocean Sci, Bangalore 560012, Karnataka, India.
[Roca, Remy] OMP LEGOS, F-31400 Toulouse, France.
RP Roca, R (reprint author), OMP LEGOS, 14 Av Edouard Belin, F-31400 Toulouse, France.
EM Remy.Roca@legos.obs-mip.fr
RI Kidd, Christopher/H-9910-2014
NR 0
TC 2
Z9 2
U1 1
U2 5
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 0035-9009
J9 Q J ROY METEOR SOC
JI Q. J. R. Meteorol. Soc.
PD APR
PY 2013
VL 139
IS 673
SI SI
BP 841
EP 841
DI 10.1002/qj.2201
PN B
PG 1
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 164FG
UT WOS:000320393800001
ER
PT J
AU Kacimi, S
Viltard, N
Kirstetter, PE
AF Kacimi, Sahra
Viltard, Nicolas
Kirstetter, Pierre-Emmanuel
TI A new methodology for rain identification from passive microwave data in
the Tropics using neural networks
SO QUARTERLY JOURNAL OF THE ROYAL METEOROLOGICAL SOCIETY
LA English
DT Article
DE passive microwave; neural networks; Probability of Detection; bias;
Bayesian inversion; rainfall estimation
ID PRECIPITATION ESTIMATION; RETRIEVAL ALGORITHMS; PROFILING ALGORITHM;
TRMM; SENSORS; CLOUDS; RADAR; WATER; LAND
AB The detection of rainfall remains a challenge for the monitoring of precipitation from space. A methodology is presented to identify rain events from spaceborne passive microwave data using neural networks. We focus on BRAIN, the algorithm that provides instantaneous quantitative precipitation estimates at the surface, based on the MADRAS radiometer onboard the Megha-Tropiques satellite. A version of BRAIN using data from the Tropical Rainfall Measuring Mission (TRMM) Microwave Imager (TMI) has been used to compare several multilayer perceptrons (MLP) trained on different combinations of TMI brightness temperatures with the conventional GSCAT-2 algorithm approach used for rainfall detection. These classifiers were compared at a global scale to reference values from the TRMM Precipitation Radar (PR). They were also compared to ground measurements using two 1 degrees x 1 degrees dense rain-gauge networks from different climatic zones in West Africa to assess the inFLuence of rainfall types. At the global scale the MLPs provide better Probability of Detection than the GSCAT-2 decision tree but tend to have a higher False Alarm Rate. While no unique solution exists given the strong regional dependence of the classifiers' performances, the screen based on the 19, 21 and 85 GHz channels provides the best detection results at the instantaneous scales. As to accumulated rainfall, the screen that exhibits the lower bias relative to the PR makes use of the 37 and 85 GHz channels. The evaluation over West Africa using 10 years of TRMM overpasses shows that MLPs are in better agreement with both the PR and the gauges than GSCAT-2. The MLP trained on the 37 and 85 GHz channels increases the Probability of Detection by nearly 35% compared to the former screening over the two studied regions. Better results are obtained in the case of organized systems. Copyright (c) 2013 Royal Meteorological Society
C1 [Kacimi, Sahra] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Viltard, Nicolas] Univ Versailles, CNRS INSU, LATMOS IPSL, Guyancourt, France.
[Kirstetter, Pierre-Emmanuel] NOAA, Natl Severe Storms Lab, Norman, OK 73069 USA.
RP Kacimi, S (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr,MS 300-243, Pasadena, CA 91109 USA.
EM sahra.kacimi@jpl.nasa.gov
RI Kirstetter, Pierre/E-2305-2013; Measurement, Global/C-4698-2015
OI Kirstetter, Pierre/0000-0002-7381-0229;
NR 27
TC 4
Z9 4
U1 0
U2 5
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 0035-9009
J9 Q J ROY METEOR SOC
JI Q. J. R. Meteorol. Soc.
PD APR
PY 2013
VL 139
IS 673
SI SI
BP 912
EP 922
DI 10.1002/qj.2114
PN B
PG 11
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 164FG
UT WOS:000320393800007
ER
PT J
AU Holdaway, D
Thuburn, J
Wood, N
AF Holdaway, D.
Thuburn, J.
Wood, N.
TI Comparison of Lorenz and Charney-Phillips vertical discretisations for
dynamics-boundary layer coupling. Part I: Steady states
SO QUARTERLY JOURNAL OF THE ROYAL METEOROLOGICAL SOCIETY
LA English
DT Article
DE physics-dynamics coupling; steady-state boundary layer; vertical
staggering; NWP
ID EQUATION ATMOSPHERIC MODELS; OPTIMAL REPRESENTATION; PHYSICAL
PARAMETERIZATIONS; DISCRETIZATIONS; PARAMETRIZATIONS; SENSITIVITY;
PARALLEL; SCHEMES; SPLIT; CORE
AB Accurate coupling between the resolved-scale dynamics and the parametrised physics is essential for accurate modelling of the atmosphere. Previous emphasis has been on the temporal aspects of this so-called physics-dynamics coupling problem, with little attention on the spatial aspects. When designing a model for numerical weather prediction there is a choice for how to vertically arrange the predicted variables, namely the Lorenz and Charney-Phillips grids, and there is ongoing debate as to which is the optimal. The Charney-Phillips grid is considered good for capturing the potential vorticity dynamics and wave propagation, whereas the Lorenz grid is more suitable for conservation. However the Lorenz grid supports a computational mode. It is argued here that the Lorenz grid is preferred for modelling the stably stratified boundary layer. This presents the question: which grid will produce more accurate results when coupling the large-scale dynamics to the stably stratified planetary boundary layer? The question is addressed by examining the ability of both the Lorenz and Charney-Phillips grids to capture the steady state of a set of equations that simultaneously represents both large-scale dynamics and the planetary boundary layer. The results show that the Charney-Phillips grid is able to capture accurately the steady boundary-layer solution provided the Richardson number is calculated without vertically averaging the shear. Averaging the shear suppresses the negative feedback of the shear on the diffusion coefficient; the positive feedback, via the vertical gradient of potential temperature, then leads to the formation of unrealistic step-like features. Copyright (c) 2012 Royal Meteorological Society
C1 [Holdaway, D.; Thuburn, J.] Univ Exeter, Coll Engn Math & Phys Sci, Exeter EX4 4QJ, Devon, England.
[Holdaway, D.] NASA, Goddard Space Flight Ctr, Global Modeling & Assimilat Off, Greenbelt, MD 20771 USA.
[Wood, N.] Met Off, Exeter, Devon, England.
RP Holdaway, D (reprint author), NASA, Goddard Space Flight Ctr, Code 610-1, Greenbelt, MD 20771 USA.
EM dan.holdaway@nasa.gov
RI Holdaway, Daniel/Q-5198-2016
OI Holdaway, Daniel/0000-0002-3672-2588
FU EPSRC; Met Office under Industrial CASE partnership
FX The lead author wishes to thank the EPSRC and the Met Office for funding
this work under an Industrial CASE partnership. Further thanks are due
to the dynamics research group at the Met Office for providing access to
their expertise.
NR 35
TC 0
Z9 1
U1 1
U2 9
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 0035-9009
J9 Q J ROY METEOR SOC
JI Q. J. R. Meteorol. Soc.
PD APR
PY 2013
VL 139
IS 673
SI SI
BP 1073
EP 1086
DI 10.1002/qj.2016
PN B
PG 14
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 164FG
UT WOS:000320393800019
ER
PT J
AU Holdaway, D
Thuburn, J
Wood, N
AF Holdaway, D.
Thuburn, J.
Wood, N.
TI Comparison of Lorenz and Charney-Phillips vertical discretisations for
dynamics-boundary layer coupling. Part II: Transients
SO QUARTERLY JOURNAL OF THE ROYAL METEOROLOGICAL SOCIETY
LA English
DT Article
DE physics-dynamics coupling; computational mode; eigenmodes; atmospheric
waves
ID OPTIMAL REPRESENTATION; ATMOSPHERIC MODELS; DISCRETIZATIONS
AB A numerical comparison of the Lorenz and Charney-Phillips vertical grids for capturing the steady state of a set of equations that models the large-scale dynamics of the atmosphere and the planetary boundary layer (Part I of this article) has revealed important differences between the grids. Due to suppression of a negative feedback, Charney-Phillips grids that involve averaging of shear in the boundary-layer terms are not able to capture the structure of the boundary layer accurately. The Lorenz grid performs well in terms of capturing the boundary layer on its own, but the Charney-Phillips grids that use averaging of potential temperature gradient are generally preferred once dynamics are included. Any finite-difference approximation of the problem must be capable of accurately representing both the steady-state and time-dependent parts of the solution. In this Part II of the article, the ability of the Lorenz and Charney-Phillips configurations to capture the transient part of the system is considered. The configurations are compared in terms of their ability to capture the eigenmodes of the solution. Full comparison between Lorenz and Charney-Phillips grids is limited by non-normality of the linearised system, associated with the boundary layer. The Lorenz grid computational mode is examined. The structure is modified by the boundary layer but it still exists. For the modes that could be accurately examined, it is found that both grids perform well in terms of capturing spatial and temporal mode structure. Some Lorenz grid modes are identified that have spurious computational mode-like behaviour occurring near the top of the boundary layer. Copyright (c) 2012 Royal Meteorological Society
C1 [Holdaway, D.; Thuburn, J.] Univ Exeter, Coll Engn Math & Phys Sci, Exeter EX4 4QJ, Devon, England.
[Holdaway, D.] NASA, Goddard Space Flight Ctr, Global Modeling & Assimilat Off, Greenbelt, MD 20771 USA.
[Wood, N.] Met Off, Exeter, Devon, England.
RP Holdaway, D (reprint author), NASA, Goddard Space Flight Ctr, Code 610-1, Greenbelt, MD 20771 USA.
EM dan.holdaway@nasa.gov
RI Holdaway, Daniel/Q-5198-2016
OI Holdaway, Daniel/0000-0002-3672-2588
FU EPSRC; Met Office under Industrial CASE partnership
FX The lead author wishes to thank the EPSRC and the Met Office for funding
this work under an Industrial CASE partnership. Further thanks are due
to the dynamics research group at the Met Office for providing access to
their expertise.
NR 20
TC 1
Z9 2
U1 0
U2 5
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 0035-9009
J9 Q J ROY METEOR SOC
JI Q. J. R. Meteorol. Soc.
PD APR
PY 2013
VL 139
IS 673
SI SI
BP 1087
EP 1098
DI 10.1002/qj.2017
PN B
PG 12
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 164FG
UT WOS:000320393800020
ER
PT J
AU Ericson, KL
Cooper, BR
Peels, ME
Deng, Y
Smith, SM
Coburn, SP
AF Ericson, Karen Louise
Cooper, B. R.
Peels, M. E.
Deng, Y.
Smith, S. M.
Coburn, S. P.
TI Application of Urine Metabolomics to Probe the Effects of Long-Term Bed
Rest as a Model for Spaceflight
SO FASEB JOURNAL
LA English
DT Meeting Abstract
CT Joint Annual Meeting of the ASPET/BPS at Experimental Biology (EB)
CY APR 20-24, 2013
CL Boston, MA
SP ASPET, British Pharmacol Soc (BPS)
C1 [Ericson, Karen Louise; Peels, M. E.; Deng, Y.; Coburn, S. P.] Indiana Univ Purdue Univ, Ft Wayne, IN 46805 USA.
[Cooper, B. R.] Purdue Univ, Bindley Biosci, W Lafayette, IN 47907 USA.
[Smith, S. M.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA.
NR 0
TC 0
Z9 0
U1 0
U2 1
PU FEDERATION AMER SOC EXP BIOL
PI BETHESDA
PA 9650 ROCKVILLE PIKE, BETHESDA, MD 20814-3998 USA
SN 0892-6638
J9 FASEB J
JI Faseb J.
PD APR
PY 2013
VL 27
MA lb311
PG 1
WC Biochemistry & Molecular Biology; Biology; Cell Biology
SC Biochemistry & Molecular Biology; Life Sciences & Biomedicine - Other
Topics; Cell Biology
GA 157GG
UT WOS:000319883505456
ER
PT J
AU Heer, M
Buehlmeier, J
Smith, SM
Baecker, N
Frings-Meuthen, P
AF Heer, Martina
Buehlmeier, Judith
Smith, Scott M.
Baecker, Natalie
Frings-Meuthen, Petra
TI KHCO3 Prevents Increase in Bone Resorption with High Protein in Bed Rest
(MEP Study)
SO FASEB JOURNAL
LA English
DT Meeting Abstract
CT Joint Annual Meeting of the ASPET/BPS at Experimental Biology (EB)
CY APR 20-24, 2013
CL Boston, MA
SP ASPET, British Pharmacol Soc (BPS)
C1 [Heer, Martina] Profil, Nutr Sci, Neuss, Germany.
[Heer, Martina; Buehlmeier, Judith; Baecker, Natalie] Univ Bonn, IEL Nutr Physiol, Bonn, Germany.
[Buehlmeier, Judith; Frings-Meuthen, Petra] DLR, Inst Aerosp Med, Cologne, Germany.
[Smith, Scott M.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA.
NR 0
TC 0
Z9 0
U1 0
U2 1
PU FEDERATION AMER SOC EXP BIOL
PI BETHESDA
PA 9650 ROCKVILLE PIKE, BETHESDA, MD 20814-3998 USA
SN 0892-6638
J9 FASEB J
JI Faseb J.
PD APR
PY 2013
VL 27
MA 615.15
PG 1
WC Biochemistry & Molecular Biology; Biology; Cell Biology
SC Biochemistry & Molecular Biology; Life Sciences & Biomedicine - Other
Topics; Cell Biology
GA 156YK
UT WOS:000319860505547
ER
PT J
AU Morgan, JLL
Crucian, BE
Sams, CF
Smith, SM
Zwart, SR
AF Morgan, Jennifer L. L.
Crucian, Brian E.
Sams, Clarence F.
Smith, Scott M.
Zwart, Sara R.
TI The Effects of High Dietary Iron and Radiation Exposure on Markers of
Oxidative Stress and Immune Status of Rats
SO FASEB JOURNAL
LA English
DT Meeting Abstract
CT Joint Annual Meeting of the ASPET/BPS at Experimental Biology (EB)
CY APR 20-24, 2013
CL Boston, MA
SP ASPET, British Pharmacol Soc (BPS)
C1 [Morgan, Jennifer L. L.] NASA, ORAU, Houston, TX USA.
[Crucian, Brian E.; Sams, Clarence F.; Smith, Scott M.] NASA, Houston, TX USA.
[Zwart, Sara R.] NASA, USRA, Houston, TX USA.
NR 0
TC 0
Z9 0
U1 0
U2 1
PU FEDERATION AMER SOC EXP BIOL
PI BETHESDA
PA 9650 ROCKVILLE PIKE, BETHESDA, MD 20814-3998 USA
SN 0892-6638
J9 FASEB J
JI Faseb J.
PD APR
PY 2013
VL 27
MA 866.4
PG 1
WC Biochemistry & Molecular Biology; Biology; Cell Biology
SC Biochemistry & Molecular Biology; Life Sciences & Biomedicine - Other
Topics; Cell Biology
GA 156YK
UT WOS:000319860504284
ER
PT J
AU Serrador, JM
Falvo, MJ
Maracaja, L
Blatt, MM
Caine, TL
Stenger, MB
Platts, S
Knapp, CF
Evans, JM
AF Serrador, Jorge M.
Falvo, Michael J.
Maracaja, Luiz
Blatt, Melissa M.
Caine, Timothy L.
Stenger, Michael B.
Platts, Steven
Knapp, Charles F.
Evans, Joyce M.
TI Acute Hypovolemia Does Not Affect Dynamic Cerebral Autoregulation in
Humans
SO FASEB JOURNAL
LA English
DT Meeting Abstract
CT Joint Annual Meeting of the ASPET/BPS at Experimental Biology (EB)
CY APR 20-24, 2013
CL Boston, MA
SP ASPET, British Pharmacol Soc (BPS)
C1 [Serrador, Jorge M.; Falvo, Michael J.; Blatt, Melissa M.] VA New Jersey Healthcare Syst, WRIISC, E Orange, NJ USA.
[Serrador, Jorge M.; Falvo, Michael J.] Univ Med & Dent New Jersey, New Jersey Med Sch, Newark, NJ 07103 USA.
[Maracaja, Luiz] Suny Downstate Med Ctr, Brooklyn, NY 11203 USA.
[Caine, Timothy L.; Stenger, Michael B.; Platts, Steven] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA.
[Knapp, Charles F.; Evans, Joyce M.] Univ Kentucky, Lexington, KY USA.
NR 0
TC 0
Z9 0
U1 0
U2 1
PU FEDERATION AMER SOC EXP BIOL
PI BETHESDA
PA 9650 ROCKVILLE PIKE, BETHESDA, MD 20814-3998 USA
SN 0892-6638
J9 FASEB J
JI Faseb J.
PD APR
PY 2013
VL 27
MA 925.12
PG 1
WC Biochemistry & Molecular Biology; Biology; Cell Biology
SC Biochemistry & Molecular Biology; Life Sciences & Biomedicine - Other
Topics; Cell Biology
GA 156YK
UT WOS:000319860506194
ER
PT J
AU Smith, SM
Sceppa, CC
O'Brien, KO
Abrams, SA
Gillman, P
Zwart, SR
Wastney, ME
AF Smith, Scott M.
Sceppa, Carmen Casteneda
O'Brien, Kimberly O.
Abrams, Steven A.
Gillman, Patti
Zwart, Sara R.
Wastney, Meryl E.
TI Calcium Kinetics during Bed Rest with Artificial Gravity and Exercise
Countermeasures
SO FASEB JOURNAL
LA English
DT Meeting Abstract
CT Joint Annual Meeting of the ASPET/BPS at Experimental Biology (EB)
CY APR 20-24, 2013
CL Boston, MA
SP ASPET, British Pharmacol Soc (BPS)
C1 [Smith, Scott M.] NASA, JSC, Houston, TX USA.
[Sceppa, Carmen Casteneda] Northeastern Univ, Boston, MA 02115 USA.
[Sceppa, Carmen Casteneda] Tufts Univ, Boston, MA 02111 USA.
[O'Brien, Kimberly O.] Cornell Univ, Ithaca, NY USA.
[Abrams, Steven A.] Baylor Coll Med, Houston, TX 77030 USA.
[Gillman, Patti] NASA, EASI, Houston, TX USA.
[Zwart, Sara R.] NASA, USRA, Houston, TX USA.
[Wastney, Meryl E.] Metab Modeling, W Lafayette, IN USA.
NR 0
TC 0
Z9 0
U1 1
U2 5
PU FEDERATION AMER SOC EXP BIOL
PI BETHESDA
PA 9650 ROCKVILLE PIKE, BETHESDA, MD 20814-3998 USA
SN 0892-6638
J9 FASEB J
JI Faseb J.
PD APR
PY 2013
VL 27
MA 233.6
PG 1
WC Biochemistry & Molecular Biology; Biology; Cell Biology
SC Biochemistry & Molecular Biology; Life Sciences & Biomedicine - Other
Topics; Cell Biology
GA 156YK
UT WOS:000319860500140
ER
PT J
AU Wotring, VE
AF Wotring, Virginia E.
TI Effects of Radiation Exposure and Dietary Iron on Liver Metabolic Gene
Expression
SO FASEB JOURNAL
LA English
DT Meeting Abstract
CT Joint Annual Meeting of the ASPET/BPS at Experimental Biology (EB)
CY APR 20-24, 2013
CL Boston, MA
SP ASPET, British Pharmacol Soc (BPS)
C1 [Wotring, Virginia E.] NASA, Houston, TX USA.
NR 0
TC 0
Z9 0
U1 0
U2 0
PU FEDERATION AMER SOC EXP BIOL
PI BETHESDA
PA 9650 ROCKVILLE PIKE, BETHESDA, MD 20814-3998 USA
SN 0892-6638
J9 FASEB J
JI Faseb J.
PD APR
PY 2013
VL 27
MA 1180.7
PG 1
WC Biochemistry & Molecular Biology; Biology; Cell Biology
SC Biochemistry & Molecular Biology; Life Sciences & Biomedicine - Other
Topics; Cell Biology
GA 156YK
UT WOS:000319860503268
ER
PT J
AU Zwart, SR
Morgan, JLL
Smith, SM
AF Zwart, Sara R.
Morgan, Jennifer L. L.
Smith, Scott M.
TI Risk of Oxidative Damage and Bone Resorption from Increased Iron Stores
during Space Flight
SO FASEB JOURNAL
LA English
DT Meeting Abstract
CT Joint Annual Meeting of the ASPET/BPS at Experimental Biology (EB)
CY APR 20-24, 2013
CL Boston, MA
SP ASPET, British Pharmacol Soc (BPS)
C1 [Zwart, Sara R.] USRA NASA JSC, Houston, TX USA.
[Morgan, Jennifer L. L.] ORAU NASA JSC, Houston, TX USA.
[Smith, Scott M.] NASA, Houston, TX USA.
NR 0
TC 0
Z9 0
U1 1
U2 5
PU FEDERATION AMER SOC EXP BIOL
PI BETHESDA
PA 9650 ROCKVILLE PIKE, BETHESDA, MD 20814-3998 USA
SN 0892-6638
J9 FASEB J
JI Faseb J.
PD APR
PY 2013
VL 27
MA 634.4
PG 1
WC Biochemistry & Molecular Biology; Biology; Cell Biology
SC Biochemistry & Molecular Biology; Life Sciences & Biomedicine - Other
Topics; Cell Biology
GA 157GG
UT WOS:000319883500648
ER
PT J
AU Kocsis, MB
Cholewiak, SA
Traylor, RM
Adelstein, BD
Hirleman, ED
Tan, HZ
AF Kocsis, Matthew B.
Cholewiak, Steven A.
Traylor, Ryan M.
Adelstein, Bernard D.
Hirleman, E. Daniel
Tan, Hong Z.
TI Discrimination of Real and Virtual Surfaces with Sinusoidal and
Triangular Gratings Using the Fingertip and Stylus
SO IEEE TRANSACTIONS ON HAPTICS
LA English
DT Article
DE Haptic texture perception; real texture; virtual texture; amplitude
discrimination
ID ADAPTING MECHANORECEPTIVE AFFERENTS; PERCEIVED INSTABILITY; TACTILE
ROUGHNESS; HAPTIC TEXTURE; MONKEY FINGERPAD; PERCEPTION; FORCE;
RESPONSES; GEOMETRY; DISPLAY
AB Two-interval two-alternative forced-choice discrimination experiments were conducted separately for sinusoidal and triangular textured surface gratings from which amplitude (i.e., height) discrimination thresholds were estimated. Participants (group sizes.n = 4 to 7) explored one of these texture types either by fingertip on real gratings (Finger real), by stylus on real gratings (Stylus real), or by stylus on virtual gratings (Stylus virtual). The real gratings were fabricated from stainless steel by an electrical discharge machining process while the virtual gratings were rendered via a programmable force-feedback device. All gratings had a 2.5-mm spatial period. On each trial, participants compared test gratings with 55, 60, 65, or 70 mu m amplitudes against a 50-mu m reference. The results indicate that discrimination thresholds did not differ significantly between sinusoidal and triangular gratings. With sinusoidal and triangular data combined, the average (mean +/- standard error) for the Stylus-real threshold (2.5 +/- 0.2 mu m) was significantly smaller (p < 0.01) than that for the Stylus-virtual condition (4.9 +/- 0.2 mu m). Differences between the Finger-real threshold (3.8 +/- 0.2 mu m) and those from the other two conditions were not statistically significant. Further studies are needed to better understand the differences in perceptual cues resulting from interactions with real and virtual gratings.
C1 [Kocsis, Matthew B.] Aircell, Broomfield, CO 80021 USA.
[Cholewiak, Steven A.] Rutgers State Univ, Dept Psychol, Piscataway, NJ 08854 USA.
[Traylor, Ryan M.] Battelle Huntsville Operat, Battelle Mem Inst, Huntsville, AL 35806 USA.
[Adelstein, Bernard D.] NASA, Ames Res Ctr, Human Syst Integrat Div, Moffett Field, CA 94035 USA.
[Hirleman, E. Daniel] Univ Calif, Sch Engn, Merced, CA 95343 USA.
[Tan, Hong Z.] Purdue Univ, Sch Elect & Comp Engn, Hapt Interface Res Lab, W Lafayette, IN 47907 USA.
RP Kocsis, MB (reprint author), Aircell, 303 S Technol Ct,Bldg A, Broomfield, CO 80021 USA.
EM mattkocsis@alumni.purdue.edu; scholewi@rutgers.edu;
ryantraylor@alumni.purdue.edu; Bernard.D.Adelstein@nasa.gov;
dhirleman@ucmerced.edu; hongtan@purdue.edu
RI Cholewiak, Steven/N-6426-2013
OI Cholewiak, Steven/0000-0003-0605-4395
FU US National Science Foundation [0098443-IIS]; NASA [NCC 2-1363]; School
of Electrical and Computer Engineering at Purdue University
FX This work was supported in part by a US National Science Foundation
Award under Grant No. 0098443-IIS, and in part by NASA under award no.
NCC 2-1363. In addition, Matthew Kocsis was partially supported by a
graduate fellowship from the School of Electrical and Computer
Engineering at Purdue University. The authors thank Drs. Susan Lederman
and Roberta Klatzky for discussions on experimental methods, Mike
Sherwood at Purdue University for his assistance with the fabrication of
the EDM samples with surface gratings, Patrick Kalita for the spectral
analysis of virtual texture gratings shown in Figs. 6 and 7, and Dr.
Michael Seaman at the University of South Carolina for providing the
extended Kruskal-Wallis tables for some of the statistical analyses.
Portions of this paper reprinted with permission from [36] and [35], (c)
2006/2007 IEEE.
NR 49
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U1 0
U2 5
PU IEEE COMPUTER SOC
PI LOS ALAMITOS
PA 10662 LOS VAQUEROS CIRCLE, PO BOX 3014, LOS ALAMITOS, CA 90720-1314 USA
SN 1939-1412
EI 2329-4051
J9 IEEE T HAPTICS
JI IEEE Trans. Haptics
PD APR-JUN
PY 2013
VL 6
IS 2
BP 181
EP 192
DI 10.1109/ToH.2012.31
PG 12
WC Computer Science, Cybernetics
SC Computer Science
GA 157EA
UT WOS:000319877500005
PM 24808302
ER
PT J
AU Hellinger, P
Travnicek, PM
Stverak, S
Matteini, L
Velli, M
AF Hellinger, Petr
Travnicek, Pavel M.
Stverak, Stepan
Matteini, Lorenzo
Velli, Marco
TI Proton thermal energetics in the solar wind: Helios reloaded
SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS
LA English
DT Article
DE solar wind; proton energetics; turbulent heating
ID VELOCITY DISTRIBUTIONS; ION-BEAMS; EQUATION; PLASMA; WAVE; 1-AU;
INSTABILITIES; ANISOTROPY; TURBULENCE; EVOLUTION
AB The proton thermal energetics in the slow solar wind between 0.3 and 1 AU is reinvestigated using the Helios 1 and 2 data, complementing a similar analysis for the fast solar wind [Hellinger et al., 2011]. The results for slow and fast solar winds are compared and discussed in the context of previous results. Protons need to be heated in the perpendicular direction with respect to the ambient magnetic field from 0.3 to 1 AU. In the parallel direction, protons need to be cooled at 0.3 AU, with a cooling rate comparable to the corresponding perpendicular heating rate; between 0.3 and 1 AU, the required cooling rate decreases until a transition to heating occurs: by 1 AU the protons require parallel heating, with a heating rate comparable to that required to sustain the perpendicular temperature. The heating/cooling rates (per unit volume) in the fast and slow solar winds are proportional to the ratio between the proton kinetic energy and the expansion time. On average, the protons need to be heated and the necessary heating rates are comparable to the energy cascade rate of the magnetohydrodynamic turbulence estimated from the stationary Kolmogorov-Yaglom law at 1 AU; however, in the expanding solar wind, the stationarity assumption for this law is questionable. The turbulent energy cascade may explain the average proton energetics (although the stationarity assumption needs to be justified) but the parallel cooling is likely related to microinstabilities connected with the structure of the proton velocity distribution function. This is supported by linear analysis based on observed data and by results of numerical simulations.
C1 [Hellinger, Petr; Travnicek, Pavel M.; Stverak, Stepan] AS CR, Astron Inst, Prague, Czech Republic.
[Hellinger, Petr; Stverak, Stepan] AS CR, Inst Atmospher Phys, Prague, Czech Republic.
[Travnicek, Pavel M.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
[Matteini, Lorenzo; Velli, Marco] Univ Florence, Dipartimento Fis & Astron, Florence, Italy.
[Matteini, Lorenzo] Univ London Imperial Coll Sci Technol & Med, London, England.
[Velli, Marco] CALTECH, Jet Prop Lab, Pasadena, CA USA.
RP Hellinger, P (reprint author), AS CR, Astron Inst, Prague, Czech Republic.
EM Petr.Hellinger@asu.cas.cz
RI Hellinger, Petr/F-5267-2014; Stverak, Stepan/F-5282-2014; Travnicek,
Pavel/G-8608-2014
OI Hellinger, Petr/0000-0002-5608-0834;
FU Grant Agency of the Czech Republic [P209/12/2023, P209/12/2041];
European Commission [284515, 263340]; [RVO:67985815]; [RVO:68378289]
FX PH, SS, and PMT acknowledge grants P209/12/2023 and P209/12/2041 of the
Grant Agency of the Czech Republic. The research leading to these
results has received funding from the European Commission's Seventh
Framework Programme (FP7) under the grant agreement SHOCK (project
number 284515, project-shock.eu) and SWIFF (project number 263340,
www.swiff.eu). This work was also supported by the projects RVO:67985815
and RVO:68378289.
NR 48
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Z9 31
U1 2
U2 20
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-9380
EI 2169-9402
J9 J GEOPHYS RES-SPACE
JI J. Geophys. Res-Space Phys.
PD APR
PY 2013
VL 118
IS 4
BP 1351
EP 1365
DI 10.1002/jgra.50107
PG 15
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 157UJ
UT WOS:000319924400001
ER
PT J
AU Turner, DL
Omidi, N
Sibeck, DG
Angelopoulos, V
AF Turner, D. L.
Omidi, N.
Sibeck, D. G.
Angelopoulos, V.
TI First observations of foreshock bubbles upstream of Earth's bow shock:
Characteristics and comparisons to HFAs
SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS
LA English
DT Article
DE Ion foreshock; Particle acceleration; Kinetic phenomena
ID DIAMAGNETIC CAVITIES UPSTREAM; HOT FLOW ANOMALIES; SOLAR-WIND;
ACCELERATION; MAGNETOPAUSE; MODEL
AB Using multipoint in situ observations upstream of Earth's bow shock from the THEMIS mission, we present the first observations of foreshock bubbles (FBs) and compare them to observations of hot flow anomalies (HFAs). FBs are recently conceptualized kinetic phenomena that can form under the commonplace condition of a rotational discontinuity in the interplanetary magnetic field interacting with backstreaming energetic ions in Earth's quasi-parallel foreshock. FBs may have remained elusive until now due to their many observational similarities to HFAs and the lack of coordinated multipoint measurements. Here we introduce identification criteria for distinguishing between HFAs and FBs using in situ observations, and use them to analyze five example events that occurred on Bastille Day (14 July) and 11-12 August 2008. Three of these events satisfy the criteria for FBs and are inconsistent with multiple criteria for HFAs. The remaining two events are consistent with the traditional picture of HFAs. Furthermore, FBs involve two converging shocks, and using these events, we demonstrate their effectiveness at particle acceleration. Considering that their formation conditions are not extraordinary, FBs may be ubiquitous at collisionless, quasi-parallel shocks in a variety of astrophysical settings.
C1 [Turner, D. L.; Angelopoulos, V.] Univ Calif Los Angeles, Dept Earth & Space Sci, Los Angeles, CA 90024 USA.
[Turner, D. L.; Angelopoulos, V.] Univ Calif Los Angeles, Inst Geophys & Planetary Phys, Los Angeles, CA 90024 USA.
[Omidi, N.] Solana Sci Inc, Solana Beach, CA USA.
[Sibeck, D. G.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Turner, DL (reprint author), Univ Calif Los Angeles, Inst Geophys & Planetary Phys, Los Angeles, CA 90024 USA.
EM drew.lawson.turner@gmail.com
RI Turner, Drew/G-3224-2012
FU NASA [NAS5-02099]; NSF [AGS-1007449]
FX D. L. Turner thanks Ferdinand Plaschke, Michael Hartinger, and Heli
Hietala for invaluable discussions, comments, questions, and
suggestions. The authors would all like to thank the entire THEMIS team
and especially the following people for providing various instrument
data: Karl-Heinz Glassmeier (spacecraft magnetometers), Jim McFadden
(ESA), and Davin Larson (SST). This work was funded under NASA contract
NAS5-02099, and N. Omidi acknowledges NSF grant AGS-1007449.
NR 39
TC 17
Z9 17
U1 0
U2 3
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0148-0227
J9 J GEOPHYS RES-SPACE
JI J. Geophys. Res-Space Phys.
PD APR
PY 2013
VL 118
IS 4
BP 1552
EP 1570
DI 10.1002/jgra.50198
PG 19
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 157UJ
UT WOS:000319924400016
ER
PT J
AU Wendel, DE
Adrian, ML
AF Wendel, D. E.
Adrian, M. L.
TI Current structure and nonideal behavior at magnetic null points in the
turbulent magnetosheath
SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS
LA English
DT Article
DE turbulence; magnetosheath; magnetic reconnection; magnetic null points
ID SOLAR-WIND PLASMA; IN-SITU EVIDENCE; KINEMATIC RECONNECTION; ALIGNED
CURRENT; MHD TURBULENCE; NEUTRAL POINTS; CURRENT SHEETS; FIELD LINES;
EVOLUTION; DISCONTINUITIES
AB The Poincare index indicates that the Cluster spacecraft tetrahedron entraps a number of 3-D magnetic nulls during an encounter with the turbulent magnetosheath. Previous researchers have found evidence for reconnection at one of the many filamentary current layers observed by Cluster in this region. We find that many of the entrained nulls are also associated with strong currents. We dissect the current structure of a pair of spiral nulls that may be topologically connected. At both nulls, we find a strong current along the spine, accompanied by a somewhat more modest current perpendicular to the spine that tilts the fan toward the axis of the spine. The current along the fan is comparable to the that along the spine. At least one of the nulls manifests a rotational flow pattern in the fan plane that is consistent with torsional spine reconnection as predicted by theory. These results emphasize the importance of examining the magnetic topology in interpreting the nature of currents and reconnection in 3-D turbulence.
C1 [Wendel, D. E.; Adrian, M. L.] NASA, Goddard Space Flight Ctr, Greenbelt, MD USA.
RP Wendel, DE (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD USA.
EM deirdre.e.wendel@nasa.gov
RI Wendel, Deirdre/D-4429-2012
OI Wendel, Deirdre/0000-0002-1925-9413
FU NASA
FX The authors wish to thank Melvyn L. Goldstein, Mats Andre, and Adolfo F.
Vi as for helpful discussions. D. E. Wendel wishes to acknowledge the
assistance of Kyoung-Joo Hwang for verification of the MVA. We wish to
acknowledge data provided by the Cluster Active Archive and thank the
FGM PI Elizabeth Lucek and the EFW PI Mats Andre and their teams for
making the data available. This research was supported by NASA funding
for the Cluster mission and for the MMS Interdisciplinary Science grant
to the Goddard Space Flight Center.
NR 73
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Z9 14
U1 0
U2 8
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-9380
EI 2169-9402
J9 J GEOPHYS RES-SPACE
JI J. Geophys. Res-Space Phys.
PD APR
PY 2013
VL 118
IS 4
BP 1571
EP 1588
DI 10.1002/jgra.50234
PG 18
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 157UJ
UT WOS:000319924400017
ER
PT J
AU Raines, JM
Gershman, DJ
Zurbuchen, TH
Sarantos, M
Slavin, JA
Gilbert, JA
Korth, H
Anderson, BJ
Gloeckler, G
Krimigis, SM
Baker, DN
McNutt, RL
Solomon, SC
AF Raines, Jim M.
Gershman, Daniel J.
Zurbuchen, Thomas H.
Sarantos, Menelaos
Slavin, James A.
Gilbert, Jason A.
Korth, Haje
Anderson, Brian J.
Gloeckler, George
Krimigis, Stamatios M.
Baker, Daniel N.
McNutt, Ralph L., Jr.
Solomon, Sean C.
TI Distribution and compositional variations of plasma ions in Mercury's
space environment: The first three Mercury years of MESSENGER
observations
SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS
LA English
DT Article
DE Mercury; exosphere; magnetosphere; plasma composition
ID SODIUM EXOSPHERE; SPATIAL-DISTRIBUTION; MAGNETIC-FIELD; MAGNETOSPHERE;
ATMOSPHERE; SURFACE; MODEL; ACCELERATION; INSTRUMENT; DEPENDENCE
AB We have analyzed measurements of planetary ions near Mercury made by the MErcury Surface, Space ENvironment, GEochemistry, and Ranging (MESSENGER) Fast Imaging Plasma Spectrometer (FIPS) over the first three Mercury years of orbital observations (25 March 2011 through 31 December 2011). We determined the composition and spatial distributions of the most abundant species in the regions sampled by the MESSENGER spacecraft during that period. In particular, we here focus on altitude dependence and relative abundances of species in a variety of spatial domains. We used observed density as a proxy for ambient plasma density, because of limitations to the FIPS field of view. We find that the average observed density is 3.9 x 10-2cm-3 for He2+, 3.4 x 10-4cm-3 for He+, 8.0 x 10-4cm-3 for O+-group ions, and 5.1 x 10-3cm-3 for Na+-group ions. Na+-group ions are particularly enhanced over other planetary ions (He+ and O+ group) in the northern magnetospheric cusp (by a factor of similar to 2.0) and in the premidnight sector on the nightside (by a factor of similar to 1.6). Within 30 degrees of the equator, the average densities of all planetary ions are depressed at the subsolar point relative to the dawn and dusk terminators. The effect is largest for Na+-group ions, which are 49% lower in density at the subsolar point than at the terminators. This depression could be an effect of the FIPS energy threshold. The three planetary ion species considered show distinct dependences on altitude and local time. The Na+ group has the smallest e-folding height at all dayside local times, whereas He+ has the largest. At the subsolar point, the e-folding height for Na+-group ions is 590km, and that for the O+ group and He+ is 1100km. On the nightside and within 750km of the geographic equator, Na+-group ions are enhanced in the premidnight sector. This enhancement is consistent with nonadiabatic motion and may be observational evidence that nonadiabatic effects are important in Mercury's magnetosphere.
C1 [Raines, Jim M.; Gershman, Daniel J.; Zurbuchen, Thomas H.; Slavin, James A.; Gilbert, Jason A.; Gloeckler, George] Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA.
[Sarantos, Menelaos] NASA, Goddard Space Flight Ctr, Heliophys Sci Div, Greenbelt, MD 20771 USA.
[Sarantos, Menelaos] Univ Maryland Baltimore Cty, Goddard Planetary Heliophys Inst, Baltimore, MD 21228 USA.
[Korth, Haje; Anderson, Brian J.; Krimigis, Stamatios M.; McNutt, Ralph L., Jr.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD USA.
[Krimigis, Stamatios M.] Acad Athens, Off Space Res & Technol, Athens, Greece.
[Baker, Daniel N.] Univ Colorado, Atmospher & Space Phys Lab, Boulder, CO 80309 USA.
[Solomon, Sean C.] Carnegie Inst Sci, Dept Terr Magnetism, Washington, DC USA.
[Solomon, Sean C.] Columbia Univ, Lamont Doherty Earth Observ, Palisades, NY USA.
RP Raines, JM (reprint author), Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA.
EM jraines@umich.edu
RI Sarantos, Menelaos/H-8136-2013; Slavin, James/H-3170-2012; McNutt,
Ralph/E-8006-2010; Gilbert, Jason/I-9020-2012
OI Slavin, James/0000-0002-9206-724X; McNutt, Ralph/0000-0002-4722-9166;
Gilbert, Jason/0000-0002-3182-7014
FU NASA's Graduate Student Research Program; MESSENGER mission; NASA
Discovery Program [NAS5-97271, NASW-00002]
FX This work was supported by NASA's Graduate Student Research Program and
the MESSENGER mission. The MESSENGER project is supported by the NASA
Discovery Program under contracts NAS5-97271 to The Johns Hopkins
University Applied Physics Laboratory and NASW-00002 to the Carnegie
Institution of Washington. NASA's Astrophysics Data System has been used
extensively for this work. J.M.R. thanks Jonathan W. Thomas for
designing and programming FIPS software libraries and Mark O. Stakhiv
for suggesting one of the key visualizations used in this work.
NR 64
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U1 1
U2 16
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0148-0227
J9 J GEOPHYS RES-SPACE
JI J. Geophys. Res-Space Phys.
PD APR
PY 2013
VL 118
IS 4
BP 1604
EP 1619
DI 10.1029/2012JA018073
PG 16
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 157UJ
UT WOS:000319924400019
ER
PT J
AU Glocer, A
Fok, M
Meng, X
Toth, G
Buzulukova, N
Chen, S
Lin, K
AF Glocer, A.
Fok, M.
Meng, X.
Toth, G.
Buzulukova, N.
Chen, S.
Lin, K.
TI CRCM+BATS-R-US two-way coupling
SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS
LA English
DT Article
DE magnetosphere; Ring Current; MHD; Modeling; Model Coupling
ID BLOCK-ADAPTIVE GRIDS; RING CURRENT; INNER MAGNETOSPHERE; GEOMAGNETIC
STORMS; NOSE STRUCTURES; FIELD MODEL; MAGNETOHYDRODYNAMICS; SIMULATION;
PROTONS; SHEET
AB We present the coupling methodology and validation of a fully coupled inner and global magnetosphere code using the infrastructure provided by the Space Weather Modeling Framework (SWMF). In this model, the Comprehensive Ring Current Model (CRCM) represents the inner magnetosphere, while the BlockAdaptiveTree SolarWind RoeType Upwind Scheme (BATSRUS) represents the global magnetosphere. The combined model is a global magnetospheric code with a realistic ring current and consistent electric and magnetic fields. The computational performance of the model was improved to surpass realtime execution by the use of the Message Passing Interface (MPI) to parallelize the CRCM. Initial simulations under steady driving found that the coupled model resulted in a higher pressure in the inner magnetosphere and an inflated closed fieldline region as compared to simulations without innermagnetosphere coupling. Our validation effort was split into two studies. The first study examined the ability of the model to reproduce Dst for a range of events from the Geospace Environment Modeling (GEM) Dst Challenge. It also investigated the possibility of a baseline shift and compared two approaches to calculating Dst from the model. We found that the model did a reasonable job predicting Dst and SymH according to our two metrics of prediction efficiency and predicted yield. The second study focused on the specific case of the 22 July 2009 moderate geomagnetic storm. In this study, we directly compare model predictions and observations for Dst, THEMIS energy spectragrams, TWINS ENA images, and GOES 11 and 12 magnetometer data. The model did an adequate job reproducing trends in the data. Moreover, we found that composition can have a large effect on the result.
C1 [Glocer, A.; Fok, M.; Buzulukova, N.; Lin, K.] NASA, Goddard Space Flight Ctr, Geospace Phys Lab, Greenbelt, MD USA.
[Meng, X.; Toth, G.] Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA.
[Buzulukova, N.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Buzulukova, N.] NASA, Goddard Space Flight Ctr, CRESST, Greenbelt, MD 20771 USA.
[Chen, S.] Univ Space Res Assoc, Columbia, MD USA.
RP Glocer, A (reprint author), NASA, Goddard Space Flight Ctr, Geospace Phys Lab, Greenbelt, MD USA.
EM alex.glocer-1@nasa.gov
RI Glocer, Alex/C-9512-2012; Toth, Gabor/B-7977-2013; feggans,
john/F-5370-2012; Fok, Mei-Ching/D-1626-2012; Meng, Xing/A-1929-2016
OI Glocer, Alex/0000-0001-9843-9094; Toth, Gabor/0000-0002-5654-9823;
FU NASA High-End Computing (HEC) Program through the NASA Advanced
Supercomputing (NAS) Division at Ames Research Center; NASA Center for
Climate Simulation (NCCS) at Goddard Space Flight Center
FX Resources supporting this work were provided by the NASA High-End
Computing (HEC) Program through the NASA Advanced Supercomputing (NAS)
Division at Ames Research Center and the NASA Center for Climate
Simulation (NCCS) at Goddard Space Flight Center. This work was carried
out as a part of the TWINS mission, which is part of NASA's Explorer
Program.
NR 52
TC 20
Z9 20
U1 0
U2 5
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0148-0227
J9 J GEOPHYS RES-SPACE
JI J. Geophys. Res-Space Phys.
PD APR
PY 2013
VL 118
IS 4
BP 1635
EP 1650
DI 10.1002/jgra.50221
PG 16
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 157UJ
UT WOS:000319924400021
ER
PT J
AU Capossela, KM
Fabrizio, MC
Brill, RW
AF Capossela, Karen M.
Fabrizio, Mary C.
Brill, Richard W.
TI Migratory and within-estuary behaviors of adult Summer Flounder
(Paralichthys dentatus) in a lagoon system of the southern mid-Atlantic
Bight
SO FISHERY BULLETIN
LA English
DT Article
ID LOWER CHESAPEAKE BAY; JUVENILE SUMMER; NEW-JERSEY; WINTER FLOUNDER;
PSEUDOPLEURONECTES-AMERICANUS; ULTRASONIC TELEMETRY; ACOUSTIC TELEMETRY;
GROWTH LIMITATION; HABITAT DYNAMICS; 2 TEMPERATURES
AB We monitored the movements of 45 adult Summer Flounder (Paralichthys dentatus) between June 2007 and July 2008 through the use of passive acoustic telemetry to elucidate migratory and within-estuary behaviors in a lagoon system of the southern mid-Atlantic Bight. Between 8 June and 10 October 2007, fish resided primarily in the deeper (>3 m) regions of the system and exhibited low levels of large-scale (100s of meters) activity. Mean residence time within this estuarine lagoon system was conservatively estimated to be 130 days (range: 18-223 days), which is 1.5 times longer than the residence time previously reported for Summer Flounder in a similar estuarine habitat similar to 250 km to the north. The majority of fish remained within the lagoon system until mid-October, although some fish dispersed earlier and some of them appeared to disperse temporarily (i.e., exited the system for at least 14 consecutive days before returning). Larger fish were more likely to disperse before mid-October than smaller fish and may have moved to other estuaries or the inner continental shelf. Fish that dispersed after mid-October were more likely to return to the lagoon system the following spring than were fish that dispersed before mid-October. In 2008, fish returned to the system between 7 February and 7 April. Dispersals and returns most closely followed seasonal changes in mean water temperature, but photoperiod and other factors also may have played a role in large-scale movements of Summer Flounder.
C1 [Capossela, Karen M.; Fabrizio, Mary C.] Virginia Inst Marine Sci, Coll William & Mary, Dept Fisheries Sci, Gloucester Point, VA 23062 USA.
[Brill, Richard W.] NOAA, James J Howard Marine Sci Lab, Northeast Fisheries Sci Ctr, Natl Marine Fisheries Serv, Highlands, NJ 07732 USA.
RP Capossela, KM (reprint author), Maryland Dept Nat Resources, 301 Marine Acad Dr, Stevensville, MD 21666 USA.
EM kcapossela@dnr.state.md.us
OI Fabrizio, Mary/0000-0002-6115-5490
FU Oceanside Conservation Co., Inc.; Eastern Shore Graduate Research Grant
FX We thank the following individuals for their assistance with this study:
P. Bushnell, D. Gauthier, M. Henderson, J. Smith, and L. Smith. We
acknowledge M. Luckenbach, S. Fate, R. Bonniwell, and the support staff
of the Virginia Institute of Marine Science Eastern Shore Laboratory. We
also thank T. Targett for his comments on earlier drafts of this
manuscript and D. Fox for sharing detections from Delaware Bay. Funding
for this project was provided by the Oceanside Conservation Co., Inc.,
Student Research Grant, and the Eastern Shore Graduate Research Grant.
This is contribution 3251 from the Virginia Institute of Marine Science,
College of William & Mary.
NR 55
TC 11
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U1 1
U2 22
PU NATL MARINE FISHERIES SERVICE SCIENTIFIC PUBL OFFICE
PI SEATTLE
PA 7600 SAND POINT WAY NE BIN C15700, SEATTLE, WA 98115 USA
SN 0090-0656
EI 1937-4518
J9 FISH B-NOAA
JI Fish. Bull.
PD APR
PY 2013
VL 111
IS 2
BP 189
EP 201
DI 10.7755/FB.111.2.6
PG 13
WC Fisheries
SC Fisheries
GA 149HQ
UT WOS:000319310000006
ER
PT J
AU Taylor, RG
Scanlon, B
Doll, P
Rodell, M
van Beek, R
Wada, Y
Longuevergne, L
Leblanc, M
Famiglietti, JS
Edmunds, M
Konikow, L
Green, TR
Chen, JY
Taniguchi, M
Bierkens, MFP
MacDonald, A
Fan, Y
Maxwell, RM
Yechieli, Y
Gurdak, JJ
Allen, DM
Shamsudduha, M
Hiscock, K
Yeh, PJF
Holman, I
Treidel, H
AF Taylor, Richard G.
Scanlon, Bridget
Doell, Petra
Rodell, Matt
van Beek, Rens
Wada, Yoshihide
Longuevergne, Laurent
Leblanc, Marc
Famiglietti, James S.
Edmunds, Mike
Konikow, Leonard
Green, Timothy R.
Chen, Jianyao
Taniguchi, Makoto
Bierkens, Marc F. P.
MacDonald, Alan
Fan, Ying
Maxwell, Reed M.
Yechieli, Yossi
Gurdak, Jason J.
Allen, Diana M.
Shamsudduha, Mohammad
Hiscock, Kevin
Yeh, Pat J. -F.
Holman, Ian
Treidel, Holger
TI Ground water and climate change
SO NATURE CLIMATE CHANGE
LA English
DT Review
ID MURRAY-DARLING BASIN; UNITED-STATES; LAND-SURFACE; HIGH-PLAINS;
RECHARGE; IRRIGATION; AUSTRALIA; IMPACT; MODEL; RESOURCES
AB As the world's largest distributed store of fresh water, ground water plays a central part in sustaining ecosystems and enabling human adaptation to climate variability and change. The strategic importance of ground water for global water and food security will probably intensify under climate change as more frequent and intense climate extremes (droughts and floods) increase variability in precipitation, soil moisture and surface water. Here we critically review recent research assessing the impacts of climate on ground water through natural and human-induced processes as well as through groundwater-driven feedbacks on the climate system. Furthermore, we examine the possible opportunities and challenges of using and sustaining groundwater resources in climate adaptation strategies, and highlight the lack of groundwater observations, which, at present, limits our understanding of the dynamic relationship between ground water and climate.
C1 [Taylor, Richard G.] UCL, Dept Geog, London WC1E 6BT, England.
[Scanlon, Bridget] Univ Texas Austin, Jackson Sch Geosci, Bur Econ Geol, Austin, TX 78758 USA.
[Doell, Petra] Goethe Univ Frankfurt, Inst Phys Geog, D-60054 Frankfurt, Germany.
[Rodell, Matt] NASA, Hydrol Sci Branch, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[van Beek, Rens; Wada, Yoshihide; Bierkens, Marc F. P.] Univ Utrecht, Dept Phys Geog, NL-3508 TC Utrecht, Netherlands.
[Longuevergne, Laurent] Univ Rennes 1, Geosci Rennes, F-35042 Rennes, France.
[Leblanc, Marc] James Cook Univ, NCGRT, Sch Earth & Environm Sci, Cairns, Qld 4870, Australia.
[Famiglietti, James S.] Univ Calif Irvine, UC Ctr Hydrol Modelling, Irvine, CA 92617 USA.
[Edmunds, Mike] Univ Oxford, Sch Geog & Environm, Oxford OX1 3QY, England.
[Konikow, Leonard] US Geol Survey, Reston, VA 20192 USA.
[Green, Timothy R.] ARS, Agr Syst Res Unit, USDA, Ft Collins, CO 80526 USA.
[Chen, Jianyao] Sun Yat Sen Univ, Sch Geog & Planning, Guangzhou 510275, Guangdong, Peoples R China.
[Taniguchi, Makoto] Res Inst Humanity & Nat, Kyoto 6308047, Japan.
[MacDonald, Alan] British Geol Survey, Edinburgh EH9 3LA, Midlothian, Scotland.
[Fan, Ying] Rutgers State Univ, Dept Earth & Planetary Sci, New Brunswick, NJ 08901 USA.
[Maxwell, Reed M.] Colorado Sch Mines, Dept Geol & Geol Engn, Golden, CO 80401 USA.
[Yechieli, Yossi] Geol Survey Israel, IL-95501 Jerusalem, Israel.
[Gurdak, Jason J.] San Francisco State Univ, Dept Geosci, San Francisco, CA 94132 USA.
[Allen, Diana M.] Simon Fraser Univ, Dept Earth Sci, Burnaby, BC V5A 1S6, Canada.
[Shamsudduha, Mohammad] UCL, Inst Risk & Disaster Reduct, London WC1E 6BT, England.
[Hiscock, Kevin] Univ E Anglia, Sch Environm Sci, Norwich NR4 7TJ, Norfolk, England.
[Yeh, Pat J. -F.] UNESCO, Int Ctr Water Hazard & Risk Management ICHARM, Tsukuba, Ibaraki 1538505, Japan.
[Holman, Ian] Cranfield Univ, Environm Sci & Technol Dept, Milton Keynes MK43 0AL, Bucks, England.
[Treidel, Holger] UNESCO IHP, Div Water Sci, F-75732 Paris 15, France.
RP Taylor, RG (reprint author), UCL, Dept Geog, Mortimer St, London WC1E 6BT, England.
EM r.taylor@geog.ucl.ac.uk
RI Maxwell, Reed/D-7980-2013; Doll, Petra/A-3784-2009; YEH,
Pat/B-2758-2011; Wada, Yoshihide/F-3595-2012; Rodell,
Matthew/E-4946-2012; James Cook University, TESS/B-8171-2012; TropWATER,
Research ID/P-1401-2014; Allen, Diana/A-4215-2010; Taniguchi,
Makoto/E-3335-2012; Longuevergne, Laurent /F-4641-2010; van Beek,
Rens/B-4904-2014
OI Holman, Ian/0000-0002-5263-7746; Maxwell, Reed/0000-0002-1364-4441;
Doll, Petra/0000-0003-2238-4546; YEH, Pat/0000-0001-7629-3362; Wada,
Yoshihide/0000-0003-4770-2539; Rodell, Matthew/0000-0003-0106-7437;
Allen, Diana/0000-0003-3541-2470; Taniguchi, Makoto/0000-0001-7416-0275;
Longuevergne, Laurent /0000-0003-3169-743X; van Beek,
Rens/0000-0002-4758-108X
NR 98
TC 191
Z9 193
U1 51
U2 417
PU NATURE PUBLISHING GROUP
PI LONDON
PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND
SN 1758-678X
J9 NAT CLIM CHANGE
JI Nat. Clim. Chang.
PD APR
PY 2013
VL 3
IS 4
BP 322
EP 329
DI 10.1038/NCLIMATE1744
PG 8
WC Environmental Sciences; Environmental Studies; Meteorology & Atmospheric
Sciences
SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences
GA 150OL
UT WOS:000319400400008
ER
PT J
AU Middleton, EM
Ungar, SG
Mandl, DJ
Ong, L
Frye, SW
Campbell, PE
Landis, DR
Young, JP
Pollack, NH
AF Middleton, Elizabeth M.
Ungar, Stephen G.
Mandl, Daniel J.
Ong, Lawrence
Frye, Stuart W.
Campbell, Petya E.
Landis, David R.
Young, Joseph P.
Pollack, Nathan H.
TI The Earth Observing One (EO-1) Satellite Mission: Over a Decade in Space
SO IEEE JOURNAL OF SELECTED TOPICS IN APPLIED EARTH OBSERVATIONS AND REMOTE
SENSING
LA English
DT Article
DE Advanced Land Imager; ALI; Earth; EO-1; Hyperion; imaging spectrometer;
remote sensing
ID ADVANCED LAND IMAGER; LEAF-AREA INDEX; AUTONOMOUS SCIENCECRAFT
EXPERIMENT; PEARL RIVER ESTUARY; HYPERION DATA; HYPERSPECTRAL IMAGE;
ATMOSPHERIC CORRECTION; APPALACHIAN MOUNTAINS; CHLOROPHYLL CONTENT;
VEGETATION INDEXES
AB The Earth Observing One (EO-1) satellite was launched in November 2000 as a technology demonstration mission with an estimated 1-year lifespan. It has now successfully completed 12 years of high spatial resolution imaging operations from low Earth orbit. EO-1's two main instruments, Hyperion and the Advanced Land Imager (ALI), have both served as prototypes for new generation satellite missions. ALI, an innovative multispectral instrument, is the forerunner of the Operational Land Imager (OLI) onboard the Landsat Data Continuity Mission's (LDCM) Landsat-8 satellite, recently launched in Feb. 2013. Hyperion, a hyperspectral instrument, serves as the heritage orbital spectrometer for future global platforms, including the proposed NASA Hyperspectral Infrared Imager (HyspIRI) and the forthcoming (in 2017) German satellite, EnMAP.
This JSTARS Special Issue is dedicated to EO-1. This paper serves as an introduction to the Hyperion and ALI instruments, their capabilities, and the important contributions this mission has made to the science and technology communities. This paper also provides an overview of the EO-1 mission, including the several operational phases which have characterized its lifetime. It also briefly describes calibration and validation activities, and gives an overview of the spin-off technologies, including disaster monitoring and new Web-based tools which can be adapted for use in future missions.
C1 [Middleton, Elizabeth M.] NASA, Goddard Space Flight Ctr, Biospher Sci Lab, Greenbelt, MD 20771 USA.
[Ungar, Stephen G.] Univ Space Res Assoc, Columbia, MD 21044 USA.
[Mandl, Daniel J.] NASA, Goddard Space Flight Ctr, Software Syst Engn Branch, Greenbelt, MD 20771 USA.
[Ong, Lawrence; Pollack, Nathan H.] Syst Sci & Applicat Inc, Lanham, MD 20706 USA.
[Frye, Stuart W.; Young, Joseph P.] SGT, Greenbelt, MD 20770 USA.
[Campbell, Petya E.] Univ Maryland Baltimore Cty, Baltimore, MD 21228 USA.
[Landis, David R.] Sigma Space Corp Inc, Lanham, MD 20706 USA.
RP Middleton, EM (reprint author), NASA, Goddard Space Flight Ctr, Biospher Sci Lab, Code 618, Greenbelt, MD 20771 USA.
RI Campbell, Petya/G-4931-2013; Campbell, Petya/L-7486-2013
OI Campbell, Petya/0000-0002-0505-4951; Campbell, Petya/0000-0002-0505-4951
NR 101
TC 29
Z9 30
U1 10
U2 61
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 1939-1404
J9 IEEE J-STARS
JI IEEE J. Sel. Top. Appl. Earth Observ. Remote Sens.
PD APR
PY 2013
VL 6
IS 2
SI SI
BP 243
EP 256
DI 10.1109/JSTARS.2013.2249496
PN 1
PG 14
WC Engineering, Electrical & Electronic; Geography, Physical; Remote
Sensing; Imaging Science & Photographic Technology
SC Engineering; Physical Geography; Remote Sensing; Imaging Science &
Photographic Technology
GA 148VV
UT WOS:000319277100001
ER
PT J
AU Chien, S
Mclaren, D
Tran, D
Davies, AG
Doubleday, J
Mandl, D
AF Chien, Steve
Mclaren, David
Tran, Daniel
Davies, Ashley Gerard
Doubleday, Joshua
Mandl, Daniel
TI Onboard Product Generation on Earth Observing One: A Pathfinder for the
Proposed Hyspiri Mission Intelligent Payload Module
SO IEEE JOURNAL OF SELECTED TOPICS IN APPLIED EARTH OBSERVATIONS AND REMOTE
SENSING
LA English
DT Article
DE Cryosphere; flooding; instrument data processing; onboard processing;
thermal analysis; volcanoes
ID AUTONOMOUS SCIENCECRAFT EXPERIMENT; MERIS; EO-1
AB The proposed HyspIRI mission is evaluating a X-band Direct Broadcast capability that would enable data to be delivered to ground stations virtually as it is acquired. However the HyspIRI VSWIR and TIR instruments are expected to produce over 800 x 10(6) bits per second of data while the Direct Broadcast capability is approximately 10 x 10(6) bits per second for a similar to 80x oversubscription. In order to address this data throughput mismatch a Direct Broadcast concept called the Intelligent Payload Module (IPM) has been developed to determine which data to downlink based on both the type of surface the spacecraft is overlying and onboard processing of the data to detect events. For example, when the spacecraft is overlying polar regions it might downlink a snow/ice product. Additionally the onboard software would search for thermal signatures indicative of a volcanic event or wild fire and downlink summary information (extent, spectra) when detected.
Earth Observing One (EO-1) has served as a test bed and pathfinder for this type of onboard product generation. As part of the Autonomous Sciencecraft (ASE), EO-1 implemented in flight software the ability to analyze and develop products for a limited swath of the Hyperion hyperspectral instrument onboard the spacecraft. In a series of technology demonstrations that became part of the operational EO-1 system over 5000 science products have been generated onboard EO-1 and down linked via engineering S-band contacts, a routine automated process that continues to this day. We describe the onboard products demonstrated in EO-1 operations and show how they have paved the way for the HyspIRI Intelligent Payload Module concept.
C1 [Chien, Steve] CALTECH, Jet Prop Lab, Artificial Intelligence Lab, Pasadena, CA 91125 USA.
[Mclaren, David; Tran, Daniel; Doubleday, Joshua] CALTECH, Jet Prop Lab, Artificial Intelligence Grp, Pasadena, CA USA.
[Davies, Ashley Gerard] CALTECH, Jet Prop Lab, Earth & Space Sci Div, Pasadena, CA USA.
[Mandl, Daniel] NASA, Goddard Space Flight Ctr, Greenbelt, MD USA.
RP Chien, S (reprint author), CALTECH, Jet Prop Lab, Artificial Intelligence Lab, Pasadena, CA 91125 USA.
FU National Aeronautics and Space Administration
FX Portions of this work were performed by the Jet Propulsion Laboratory,
California Institute of Technology, under contract from the National
Aeronautics and Space Administration.
NR 20
TC 7
Z9 7
U1 0
U2 7
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 1939-1404
J9 IEEE J-STARS
JI IEEE J. Sel. Top. Appl. Earth Observ. Remote Sens.
PD APR
PY 2013
VL 6
IS 2
SI SI
BP 257
EP 264
DI 10.1109/JSTARS.2013.2249574
PN 1
PG 8
WC Engineering, Electrical & Electronic; Geography, Physical; Remote
Sensing; Imaging Science & Photographic Technology
SC Engineering; Physical Geography; Remote Sensing; Imaging Science &
Photographic Technology
GA 148VV
UT WOS:000319277100002
ER
PT J
AU Huemmrich, KF
Gamon, JA
Tweedie, CE
Campbell, PKE
Landis, DR
Middleton, EM
AF Huemmrich, Karl Fred
Gamon, John A.
Tweedie, Craig E.
Campbell, Petya K. Entcheva
Landis, David R.
Middleton, Elizabeth M.
TI Arctic Tundra Vegetation Functional Types Based on Photosynthetic
Physiology and Optical Properties
SO IEEE JOURNAL OF SELECTED TOPICS IN APPLIED EARTH OBSERVATIONS AND REMOTE
SENSING
LA English
DT Article
DE Environmental factors; ecosystems; geoscience and remote sensing;
hyperspectral imaging; remote sensing; vegetation mapping
ID CLIMATE-CHANGE; REFLECTANCE SPECTRA; GLOBAL CHANGE; CARBON-CYCLE; CO2
FLUX; ECOSYSTEMS; ALASKA; PRODUCTIVITY; RESPONSES; LICHENS
AB Non-vascular plants (lichens and mosses) are significant components of tundra landscapes and may respond to climate change differently from vascular plants affecting ecosystem carbon balance. Remote sensing provides critical tools for monitoring plant cover types, as optical signals provide a way to scale from plot measurements to regional estimates of biophysical properties, for which spatial-temporal patterns may be analyzed. Gas exchange measurements were collected for pure patches of key vegetation functional types (lichens, mosses, and vascular plants) in sedge tundra at Barrow AK. These functional types were found to have three significantly different values of light use efficiency (LUE) with values of 0.013 +/- 0.001, 0.0018 +/- 0.0002, and 0.0012 +/- 0.0001 mol C mol(-1) absorbed quanta for vascular plants, mosses and lichens, respectively. Discriminant analysis of the spectra reflectance of these patches identified five spectral bands that separated each of these vegetation functional types as well as nongreen material (bare soil, standing water, and dead leaves). These results were tested along a 100 m transect where midsummer spectral reflectance and vegetation coverage were measured at one meter intervals.
Along the transect, area-averaged canopy LUE estimated from coverage fractions of the three functional types varied widely, even over short distances. The patch-level statistical discriminant functions applied to in situ hyperspectral reflectance data collected along the transect successfully unmixed cover fractions of the vegetation functional types. The unmixing functions, developed from the transect data, were applied to 30 m spatial resolution Earth Observing-1 Hyperion imaging spectrometer data to examine variability in distribution of the vegetation functional types for an area near Barrow, AK. Spatial variability of LUE was derived from the observed functional type distributions. Across this landscape, a fivefold variation in tundra LUE was observed. LUE calculated from the functional type cover fractions was also correlated to a spectral vegetation index developed to detect vegetation chlorophyll content. The concurrence of these alternate methods suggest that hyperspectral remote sensing can distinguish functionally distinct vegetation types and can be used to develop regional estimates of photosynthetic LUE in tundra landscapes.
C1 [Huemmrich, Karl Fred; Campbell, Petya K. Entcheva] Univ Maryland Baltimore Cty, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Gamon, John A.] Univ Alberta, Edmonton, AB T6G 2R3, Canada.
[Tweedie, Craig E.] Univ Texas El Paso, El Paso, TX 79968 USA.
[Landis, David R.] Sigma Space Corp, Lanham, MD 20706 USA.
[Middleton, Elizabeth M.] NASA, Greenbelt, MD 20771 USA.
RP Huemmrich, KF (reprint author), Univ Maryland Baltimore Cty, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
EM karl.f.huemmrich@nasa.gov
RI Campbell, Petya/G-4931-2013; Campbell, Petya/L-7486-2013; Gamon,
John/A-2641-2014
OI Campbell, Petya/0000-0002-0505-4951; Campbell,
Petya/0000-0002-0505-4951; Gamon, John/0000-0002-8269-7723
FU IARC through the Desert Research Institute, Reno, Nevada, USA
FX Manuscript received February 23, 2012; revised August 03, 2012; accepted
February 27, 2013. Date of publication April 24, 2013; date of current
version May 13, 2013. Funding for the field component of this study was
provided by IARC to J. A. Gamon and K. F. Huemmrich through the Desert
Research Institute, Reno, Nevada, USA.
NR 50
TC 9
Z9 9
U1 4
U2 71
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 1939-1404
EI 2151-1535
J9 IEEE J-STARS
JI IEEE J. Sel. Top. Appl. Earth Observ. Remote Sens.
PD APR
PY 2013
VL 6
IS 2
SI SI
BP 265
EP 275
DI 10.1109/JSTARS.2013.2253446
PN 1
PG 11
WC Engineering, Electrical & Electronic; Geography, Physical; Remote
Sensing; Imaging Science & Photographic Technology
SC Engineering; Physical Geography; Remote Sensing; Imaging Science &
Photographic Technology
GA 148VV
UT WOS:000319277100003
ER
PT J
AU Campbell, PKE
Middleton, EM
Thome, KJ
Kokaly, RF
Huemmrich, KF
Lagomasino, D
Novick, KA
Brunsell, NA
AF Campbell, Petya K. Entcheva
Middleton, Elizabeth M.
Thome, Kurt J.
Kokaly, Raymond F.
Huemmrich, Karl Fred
Lagomasino, David
Novick, Kimberly A.
Brunsell, Nathaniel A.
TI EO-1 Hyperion Reflectance Time Series at Calibration and Validation
Sites: Stability and Sensitivity to Seasonal Dynamics
SO IEEE JOURNAL OF SELECTED TOPICS IN APPLIED EARTH OBSERVATIONS AND REMOTE
SENSING
LA English
DT Article
DE Earth Observing-1; eddy covariance; flux sites; forest; grassland;
Hyperion; imaging spectroscopy; Pseudo-Invariant Calibration Sites;
reflectance; remote sensing; seasonal carbon dynamics; spectral time
series; vegetation function; woodland
ID RAILROAD VALLEY PLAYA; NET ECOSYSTEM EXCHANGE; ABSORPTION FEATURES;
HYPERSPECTRAL DATA; CARBON; GRADIENT; SENSORS; FLUXES; FOREST;
RESPIRATION
AB This study evaluated Earth Observing 1 (EO-1) Hyperion reflectance time series at established calibration sites to assess the instrument stability and suitability for monitoring vegetation functional parameters. Our analysis using three pseudo-invariant calibration sites in North America indicated that the reflectance time series are devoid of apparent spectral trends and their stability consistently is within 2.5-5 percent throughout most of the spectral range spanning the 12+ year data record. Using three vegetated sites instrumented with eddy covariance towers, the Hyperion reflectance time series were evaluated for their ability to determine important variables of ecosystem function. A number of narrowband and derivative vegetation indices (VI) closely described the seasonal profiles in vegetation function and ecosystem carbon exchange (e.g., net and gross ecosystem productivity) in three very different ecosystems, including a hardwood forest and tallgrass prairie in North America, and a Miombo woodland in Africa. Our results demonstrate the potential for scaling the carbon flux tower measurements to local and regional landscape levels. The VIs with stronger relationships to the CO2 parameters were derived using continuous reflectance spectra and included wavelengths associated with chlorophyll content and/or chlorophyll fluorescence. Since these indices cannot be calculated from broadband multispectral instrument data, the opportunity to exploit these spectrometer-based VIs in the future will depend on the launch of satellites such as EnMAP and HyspIRI. This study highlights the practical utility of space-borne spectrometers for characterization of the spectral stability and uniformity of the calibration sites in support of sensor cross-comparisons, and demonstrates the potential of narrowband VIs to track and spatially extend ecosystem functional status as well as carbon processes measured at flux towers.
C1 [Campbell, Petya K. Entcheva; Huemmrich, Karl Fred] Univ Maryland Baltimore Cty, NASA, GSFC, Greenbelt, MD 20771 USA.
[Middleton, Elizabeth M.] NASA, Goddard Space Flight Ctr, Lab Biospher Sci, Greenbelt, MD 20771 USA.
[Thome, Kurt J.] NASA, Goddard Space Flight Ctr, Biospher Sci Branch, Greenbelt, MD 20771 USA.
[Kokaly, Raymond F.] USGS, Denver, CO USA.
[Lagomasino, David] Florida Int Univ, Hydrogeol Lab, Miami, FL 33199 USA.
[Novick, Kimberly A.] US Forest Serv, USDA, Coweeta Hydrol Lab, So Res Stn, Otto, NC USA.
[Brunsell, Nathaniel A.] Univ Kansas, Dept Geog, Lawrence, KS 66045 USA.
RP Campbell, PKE (reprint author), Univ Maryland Baltimore Cty, NASA, GSFC, Greenbelt, MD 20771 USA.
EM petya.campbell@nasa.gov
RI Campbell, Petya/G-4931-2013; Thome, Kurtis/D-7251-2012; Campbell,
Petya/L-7486-2013; Lagomasino, David/P-8413-2015; Kokaly,
Raymond/A-6817-2017
OI Campbell, Petya/0000-0002-0505-4951; Campbell,
Petya/0000-0002-0505-4951; Lagomasino, David/0000-0003-4008-5363;
Kokaly, Raymond/0000-0003-0276-7101
FU U.S. Department of Energy (DOE) through the Office of Biological and
Environmental Research (BER) Terrestrial Carbon Processes (TCP) program
[10509-0152, DE-FG02-00ER53015, DE-FG02-95ER62083]
FX Manuscript received March 15, 2012; revised July 20, 2012 and November
02, 2012; accepted November 25, 2012. Date of publication April 24,
2013; date of current version May 13, 2013. This work was supported by
the U.S. Department of Energy (DOE) through the Office of Biological and
Environmental Research (BER) Terrestrial Carbon Processes (TCP) program
(Grants 10509-0152, DE-FG02-00ER53015, and DE-FG02-95ER62083).
NR 53
TC 15
Z9 15
U1 1
U2 35
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 1939-1404
J9 IEEE J-STARS
JI IEEE J. Sel. Top. Appl. Earth Observ. Remote Sens.
PD APR
PY 2013
VL 6
IS 2
SI SI
BP 276
EP 290
DI 10.1109/JSTARS.2013.2246139
PN 1
PG 15
WC Engineering, Electrical & Electronic; Geography, Physical; Remote
Sensing; Imaging Science & Photographic Technology
SC Engineering; Physical Geography; Remote Sensing; Imaging Science &
Photographic Technology
GA 148VV
UT WOS:000319277100004
ER
PT J
AU Chien, S
Doubleday, J
Mclaren, D
Tran, D
Tanpipat, V
Chitradon, R
Boonya-aroonnet, S
Thanapakpawin, P
Mandl, D
AF Chien, Steve
Doubleday, Joshua
Mclaren, David
Tran, Daniel
Tanpipat, Veerachai
Chitradon, Royol
Boonya-aroonnet, Surajate
Thanapakpawin, Porranee
Mandl, Daniel
TI Monitoring Flooding in Thailand Using Earth Observing One in a Sensorweb
SO IEEE JOURNAL OF SELECTED TOPICS IN APPLIED EARTH OBSERVATIONS AND REMOTE
SENSING
LA English
DT Article
DE Flooding; hydrological modeling; in-situ sensing; space-based remote
sensing
AB The Earth Observing One (EO-1) mission has been a pathfinder in demonstrating autonomous operations paradigms. In 2010-2012 (and continuing), EO-1 has been supporting sensorweb operations to enable autonomous tracking of flooding in Thailand. In this approach, the Moderate Imaging Spectrometer (MODIS) is used to perform broad-scale monitoring to track flooding at the regional level (500 m/pixel) and EO-1 is autonomously tasked in response to alerts to acquire higher resolution (30 m/pixel) Advanced Land Imager (ALI) data. This data is then automatically processed to derive products such as surface water extent and volumetric water estimates. These products are then automatically pushed to relevant authorities in Thailand for use in damage estimation, relief efforts, and damage mitigation.
EO-1 has served as a testbed and pathfinder to this type of sensorweb operations. Beginning with EO-1, these techniques for monitoring are being extended to other space sensors (such as Radarsat-2, Landsat, Worldview-2, TRMM) and integrated with hydrological models, and integration with in-situ sensors.
C1 [Chien, Steve; Doubleday, Joshua; Mclaren, David; Tran, Daniel] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Tanpipat, Veerachai] Thaiflood Net, Remote Sensing, Bangkok, Thailand.
[Mandl, Daniel] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Chien, S (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM imatanpipat@hotmail.com
FU National Aeronautics and Space Administration
FX Portions of this work were performed by the Jet Propulsion Laboratory,
California Institute of Technology, under contract from the National
Aeronautics and Space Administration.
NR 22
TC 4
Z9 4
U1 0
U2 15
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 1939-1404
EI 2151-1535
J9 IEEE J-STARS
JI IEEE J. Sel. Top. Appl. Earth Observ. Remote Sens.
PD APR
PY 2013
VL 6
IS 2
SI SI
BP 291
EP 297
DI 10.1109/JSTARS.2013.2247974
PN 1
PG 7
WC Engineering, Electrical & Electronic; Geography, Physical; Remote
Sensing; Imaging Science & Photographic Technology
SC Engineering; Physical Geography; Remote Sensing; Imaging Science &
Photographic Technology
GA 148VV
UT WOS:000319277100005
ER
PT J
AU Mandl, D
Frye, S
Cappelaere, P
Handy, M
Policelli, F
Katjizeu, M
Van Langenhove, G
Aube, G
Saulnier, JF
Sohlberg, R
Silva, JA
Kussul, N
Skakun, S
Ungar, SG
Grossman, R
Szarzynski, J
AF Mandl, Daniel
Frye, Stuart
Cappelaere, Pat
Handy, Matthew
Policelli, Fritz
Katjizeu, McCloud
Van Langenhove, Guido
Aube, Guy
Saulnier, Jean-Francois
Sohlberg, Rob
Silva, Julie A.
Kussul, Nataliia
Skakun, Sergii
Ungar, Stephen G.
Grossman, Robert
Szarzynski, Joerg
TI Use of the Earth Observing One (EO-1) Satellite for the Namibia
SensorWeb Flood Early Warning Pilot
SO IEEE JOURNAL OF SELECTED TOPICS IN APPLIED EARTH OBSERVATIONS AND REMOTE
SENSING
LA English
DT Article
DE Earth Observing One (EO-1); Flood Early Warning; sensor systems and
applications; SensorWeb
AB The Earth Observing One (EO-1) satellite was launched in November 2000 as a one year technology demonstration mission for a variety of space technologies. After the first year, it was used as a pathfinder for the creation of SensorWebs. A SensorWeb is the integration of a variety of space, airborne and ground sensors into a loosely coupled collaborative sensor system that automatically provides useful data products. Typically, a SensorWeb is comprised of heterogeneous sensors tied together with an open messaging architecture and web services. SensorWebs provide easier access to sensor data, automated data product production and rapid data product delivery. Disasters are the perfect arena to test SensorWeb functionality since emergency workers and managers need easy and rapid access to satellite, airborne and in-situ sensor data as decision support tools. The Namibia Early Flood Warning SensorWeb pilot project was established to experiment with various aspects of sensor interoperability and SensorWeb functionality. The SensorWeb system features EO-1 data along with other data sets from such satellites as Radarsat, Terra and Aqua. Finally, the SensorWeb team began to examine how to measure economic impact of SensorWeb technology infusion. This paper describes the architecture and software components that were developed along with performance improvements that were experienced. Also, problems and challenges that were encountered are described along with a vision for future enhancements to mitigate some of the problems.
C1 [Mandl, Daniel] NASA, Goddard Space Flight Ctr, Software Syst Engn Branch, Greenbelt, MD 20771 USA.
[Frye, Stuart] SGT, Greenbelt, MD 20770 USA.
[Cappelaere, Pat] Vightel Inc, Ellicott City, MD 21043 USA.
[Handy, Matthew] NASA, Goddard Space Flight Ctr, Ground Software Syst Branch, Greenbelt, MD 20771 USA.
[Policelli, Fritz] NASA, Goddard Space Flight Ctr, Div Earth Sci, Greenbelt, MD 20771 USA.
[Katjizeu, McCloud; Van Langenhove, Guido] Minist Agr Water & Forestry, Dept Hydrol, Windhoek, Namibia.
[Aube, Guy; Saulnier, Jean-Francois] Canadian Space Agcy, St Hubert, PQ J3Y 8Y9, Canada.
[Sohlberg, Rob; Silva, Julie A.] Univ Maryland, Dept Geog Sci, College Pk, MD 20742 USA.
[Kussul, Nataliia; Skakun, Sergii] NSAU, Space Res Inst NASU, UA-03680 Kiev, Ukraine.
[Ungar, Stephen G.] NASA, Goddard Space Flight Ctr, Biospher Sci Branch, Greenbelt, MD 20771 USA.
[Grossman, Robert] Univ Chicago, Computat Inst, Searle Chem Lab, Chicago, IL 60637 USA.
[Szarzynski, Joerg] United Nations Univ, D-53113 Bonn, Germany.
RP Mandl, D (reprint author), NASA, Goddard Space Flight Ctr, Software Syst Engn Branch, Code 581, Greenbelt, MD 20771 USA.
EM daniel.j.mandl@nasa.gov
RI Kussul, Nataliia/N-8649-2014; Skakun, Sergii/E-2769-2012
OI Kussul, Nataliia/0000-0002-9704-9702; Skakun, Sergii/0000-0002-9039-0174
NR 9
TC 8
Z9 8
U1 0
U2 10
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 1939-1404
J9 IEEE J-STARS
JI IEEE J. Sel. Top. Appl. Earth Observ. Remote Sens.
PD APR
PY 2013
VL 6
IS 2
SI SI
BP 298
EP 308
DI 10.1109/JSTARS.2013.2255861
PN 1
PG 11
WC Engineering, Electrical & Electronic; Geography, Physical; Remote
Sensing; Imaging Science & Photographic Technology
SC Engineering; Physical Geography; Remote Sensing; Imaging Science &
Photographic Technology
GA 148VV
UT WOS:000319277100006
ER
PT J
AU Abrams, M
Pieri, D
Realmuto, V
Wright, R
AF Abrams, Michael
Pieri, Dave
Realmuto, Vince
Wright, Robert
TI Using EO-1 Hyperion Data as HyspIRI Preparatory Data Sets for
Volcanology Applied to Mt Etna, Italy
SO IEEE JOURNAL OF SELECTED TOPICS IN APPLIED EARTH OBSERVATIONS AND REMOTE
SENSING
LA English
DT Article
DE Hyperspectral imaging; infrared image sensors; volcanic activity
ID MOUNT-ETNA; LAVA-FLOW; INFRARED DATA; LASCAR VOLCANO; SPECTRORADIOMETER
MODIS; KILAUEA VOLCANO; FLANK ERUPTION; DOME GROWTH; RADIOMETER;
SATELLITE
AB One of the main goals of the Hyperspectral and Infrared Imager (HyspIRI) mission is to provide global observations of surface attributes at local and landscape spatial scales (tens of meters to hundreds of kilometers) to map volcanic gases and surface temperatures, which are identified as indicators of impending volcanic hazards, as well as plume ejecta which pose risks to aircraft and people and property downwind. Our project has created precursor HyspIRI data sets for volcanological analyses, using existing data over Mt. Etna, Italy. We have identified 28 EO-1 Hyperion data acquisitions, and 12 near-coincident ASTER data acquisitions, covering six eruptive periods between 2001 and 2010. These data sets provide us with 30 m hyperspectral VSWIR data and 90 m multispectral TIR data (satellite). They allowed us to examine temporal sequences of several Etnaean eruptions. We addressed the following critical questions, directly related to understanding eruption hazards: 1) What do changes in SO2 emissions tell us about a volcano's activity? How well do these measurements compare with ground-based COSPEC measurements? 2) How do we use measurements of lava flow temperature and volume to predict advances of the flow front? 3) What do changes in lava lake temperatures and energy emissions tell us about possible eruptive behavior?
C1 [Abrams, Michael; Pieri, Dave; Realmuto, Vince] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Wright, Robert] Univ Hawaii, Honolulu, HI 96822 USA.
RP Abrams, M (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
FU National Aeronautics and Space Administration
FX Manuscript received February 29, 2012; revised May 28, 2012 and July 18,
2012; accepted August 28, 2012. Date of publication March 12, 2013; date
of current version May 13, 2013. Work by Abrams, Realmuto, and Pieri was
done at the California Institute of Technology, Jet Propulsion
Laboratory, under contract with the National Aeronautics and Space
Administration.
NR 49
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Z9 9
U1 1
U2 22
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 1939-1404
J9 IEEE J-STARS
JI IEEE J. Sel. Top. Appl. Earth Observ. Remote Sens.
PD APR
PY 2013
VL 6
IS 2
SI SI
BP 375
EP 385
DI 10.1109/JSTARS.2012.2224095
PN 1
PG 11
WC Engineering, Electrical & Electronic; Geography, Physical; Remote
Sensing; Imaging Science & Photographic Technology
SC Engineering; Physical Geography; Remote Sensing; Imaging Science &
Photographic Technology
GA 148VV
UT WOS:000319277100013
ER
PT J
AU Chander, G
Angal, A
Choi, T
Xiong, XX
AF Chander, Gyanesh
Angal, Amit
Choi, Taeyoung
Xiong, Xiaoxiong
TI Radiometric Cross-Calibration of EO-1 ALI With L7 ETM+ and Terra MODIS
Sensors Using Near-Simultaneous Desert Observations
SO IEEE JOURNAL OF SELECTED TOPICS IN APPLIED EARTH OBSERVATIONS AND REMOTE
SENSING
LA English
DT Article
DE Arabia 1; EO-1 ALI and Hyperion; L7 ETM+; Libya 4; Mauritania 2;
radiometric cross-calibration; RSR; SBAF; Sudan 1; Terra MODIS
ID ADVANCED LAND IMAGER; OPTICAL SATELLITE SENSORS; ON-ORBIT; SITES;
PERFORMANCE; SAHARAN; LANDSAT-7-ETM+; SPECTROMETER; HYPERION; DESIGN
AB The Earth Observing-1 (EO-1) satellite was launched on November 21, 2000, as part of a one-year technology demonstration mission. The mission was extended because of the value it continued to add to the scientific community. EO-1 has now been operational for more than a decade, providing both multispectral and hyperspectral measurements. As part of the EO-1 mission, the Advanced Land Imager (ALI) sensor demonstrates a potential technological direction for the next generation of Landsat sensors. To evaluate the ALI sensor capabilities as a precursor to the Operational Land Imager (OLI) onboard the Landsat Data Continuity Mission (LDCM, or Landsat 8 after launch), its measured top-of-atmosphere (TOA) reflectances were compared to the well-calibrated Landsat 7 (L7) Enhanced Thematic Mapper Plus (ETM+) and the Terra Moderate Resolution Imaging Spectroradiometer (MODIS) sensors in the reflective solar bands (RSB). These three satellites operate in a near-polar, sun-synchronous orbit 705 km above the Earth's surface. EO-1 was designed to fly one minute behind L7 and approximately 30 minutes in front of Terra. In this configuration, all the three sensors can view near-identical ground targets with similar atmospheric, solar, and viewing conditions. However, because of the differences in the relative spectral response (RSR), the measured physical quantities can be significantly different while observing the same target. The cross-calibration of ALI with ETM+ and MODIS was performed using near-simultaneous surface observations based on image statistics from areas observed by these sensors over four desert sites (Libya 4, Mauritania 2, Arabia 1, and Sudan 1). The differences in the measured TOA reflectances due to RSR mismatches were compensated by using a spectral band adjustment factor (SBAF), which takes into account the spectral profile of the target and the RSR of each sensor. For this study, the spectral profile of the target comes from the near-simultaneous EO-1 Hyperion data over these sites. The results indicate that the TOA reflectance measurements for ALI agree with those of ETM+ and MODIS to within 5% after the application of SBAF.
C1 [Chander, Gyanesh] US Geol Survey, Earth Resources Observat & Sci EROS Ctr, SGT Inc, Sioux Falls, SD 57198 USA.
[Angal, Amit] Sci Syst & Applicat SSAI Inc, Lanham, MD 20706 USA.
[Choi, Taeyoung] Sigma Space Corp, Lanham, MD 20706 USA.
[Xiong, Xiaoxiong] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Chander, G (reprint author), US Geol Survey, Earth Resources Observat & Sci EROS Ctr, SGT Inc, Sioux Falls, SD 57198 USA.
EM gchander@usgs.gov
RI Richards, Amber/K-8203-2015
FU U.S. Geological Survey [G10PC00044]
FX Manuscript received March 09, 2012; revised September 03, 2012, January
23, 2013; accepted March 06, 2013. Date of publication April 04, 2013;
date of current version May 13, 2013. This work was performed under U.S.
Geological Survey contract G10PC00044.
NR 40
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Z9 5
U1 13
U2 44
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 1939-1404
J9 IEEE J-STARS
JI IEEE J. Sel. Top. Appl. Earth Observ. Remote Sens.
PD APR
PY 2013
VL 6
IS 2
SI SI
BP 386
EP 399
DI 10.1109/JSTARS.2013.2251999
PN 1
PG 14
WC Engineering, Electrical & Electronic; Geography, Physical; Remote
Sensing; Imaging Science & Photographic Technology
SC Engineering; Physical Geography; Remote Sensing; Imaging Science &
Photographic Technology
GA 148VV
UT WOS:000319277100014
ER
PT J
AU McCorkel, J
Thome, K
Ong, L
AF McCorkel, Joel
Thome, Kurtis
Ong, Lawrence
TI Vicarious Calibration of EO-1 Hyperion
SO IEEE JOURNAL OF SELECTED TOPICS IN APPLIED EARTH OBSERVATIONS AND REMOTE
SENSING
LA English
DT Article
DE Hyperion; imaging spectrometer; lunar calibration; radiometric
calibration; vicarious calibration
ID ABSOLUTE RADIOMETRIC CALIBRATION; REFLECTANCE-BASED METHOD; ON-ORBIT
CALIBRATION; IMAGING SPECTROMETER; MOON; IRRADIANCE; INSTRUMENT;
RADIANCE; AVIRIS; ASTER
AB The Hyperion imaging spectrometer on the Earth Observing-1 satellite is the first high-spatial resolution imaging spectrometer to routinely acquire science-grade data from orbit. Data gathered with this instrument needs to be quantitative and accurate in order to derive meaningful information about ecosystem properties and processes. Also, comprehensive and long-term ecological studies require these data to be comparable over time, between coexisting sensors and between generations of follow-on sensors. One method to assess the radiometric calibration is the reflectance-based approach, a common technique used for several other earth science sensors covering similar spectral regions. This work presents results of radiometric calibration of Hyperion based on the reflectance-based approach of vicarious calibration implemented by University of Arizona during 2001-2005. These results show repeatability to the 2% level and accuracy on the 3-5% level for spectral regions not affected by strong atmospheric absorption. Knowledge of the stability of the Hyperion calibration from moon observations allows for an average absolute calibration based on the reflectance-based results to be determined and applicable for the lifetime of Hyperion.
C1 [McCorkel, Joel; Thome, Kurtis] NASA, Goddard Space Flight Ctr, Sci & Explorat Directorate, Greenbelt, MD 20771 USA.
[Ong, Lawrence] NASA, Goddard Space Flight Ctr, Sci Syst & Applicat Inc, Greenbelt, MD 20771 USA.
RP McCorkel, J (reprint author), NASA, Goddard Space Flight Ctr, Sci & Explorat Directorate, Greenbelt, MD 20771 USA.
EM joel.mccorkel@nasa.gov; kurtis.thome@nasa.gov; lawrence.ong@nasa.gov
RI Thome, Kurtis/D-7251-2012; McCorkel, Joel/D-4454-2012
OI McCorkel, Joel/0000-0003-2853-2036
NR 31
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U1 4
U2 39
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 1939-1404
EI 2151-1535
J9 IEEE J-STARS
JI IEEE J. Sel. Top. Appl. Earth Observ. Remote Sens.
PD APR
PY 2013
VL 6
IS 2
SI SI
BP 400
EP 407
DI 10.1109/JSTARS.2012.2225417
PN 1
PG 8
WC Engineering, Electrical & Electronic; Geography, Physical; Remote
Sensing; Imaging Science & Photographic Technology
SC Engineering; Physical Geography; Remote Sensing; Imaging Science &
Photographic Technology
GA 148VV
UT WOS:000319277100015
ER
PT J
AU Cappelaere, P
Sanchez, S
Bernabe, S
Scuri, A
Mandl, D
Plaza, A
AF Cappelaere, Pat
Sanchez, Sergio
Bernabe, Sergio
Scuri, Antonio
Mandl, Daniel
Plaza, Antonio
TI Cloud Implementation of a Full Hyperspectral Unmixing Chain Within the
NASA Web Coverage Processing Service for EO-1
SO IEEE JOURNAL OF SELECTED TOPICS IN APPLIED EARTH OBSERVATIONS AND REMOTE
SENSING
LA English
DT Article
DE Earth Observing One (EO-1); hyperion; hyperspectral imaging; NASA
SensorWeb; spectral unmixing; Web Coverage Processing Service (WCPS)
ID IMAGERY
AB The launch of the NASA Earth Observing 1 (EO-1) platform in November 2000 marked the establishment of spaceborne hyperspectral technology for land imaging. The Hyperion sensor onboard EO-1 operates in the 0.4-2.5 micrometer spectral range, with 10 nanometer spectral resolution and 30-meter spatial resolution. Spectral unmixing has been one of the most successful approaches to analyze Hyperion data since its launch. It estimates the abundance of spectrally pure constituents (endmembers) in each observation collected by the sensor. Due to the high spectral dimensionality of Hyperion data, unmixing is a very time-consuming operation. In this paper, we develop a cloud implementation of a full hyperspectral unmixing chain made up of the following steps: 1) dimensionality reduction; 2) automatic endmember identification; and 3) fully constrained abundance estimation. The unmixing chain will be available online within the Web Coverage Processing Service (WCPS), an image processing framework that can run on the cloud, as part of the NASA SensorWeb suite of web services. The proposed implementation has been demonstrated using the EO-1 Hyperion imagery. Our experimental results with a hyperspectral scene collected over the Okavango Basin in Botswana suggest the (present and future) potential of spectral unmixing for improved exploitation of spaceborne hyperspectral data. The integration of the unmixing chain in the WCPS framework as part of the NASA SensorWeb suite of web services is just the start of an international collaboration in which many more processing algorithms will be made available to the community through this service. This paper is not so much focused on the theory and results of unmixing (widely demonstrated in other contributions) but about the process and added value of the proposed contribution for ground processing on the cloud and onboard migration of those algorithms to support the generation of low-latency products for new airborne/spaceborne missions.
C1 [Cappelaere, Pat] Vightel Corp, Ellicott City, MD 21043 USA.
[Sanchez, Sergio; Bernabe, Sergio; Plaza, Antonio] Univ Extremadura, Hyperspectral Comp Lab, Calceres 10003, Spain.
[Scuri, Antonio] Pontificia Univ Catolica Rio de Janeiro PUC Rio, Tecgraf, Rio De Janeiro, Brazil.
[Mandl, Daniel] NASA, Goddard Space Flight Ctr, Software Syst Branch, Greenbelt, MD 20771 USA.
RP Cappelaere, P (reprint author), Vightel Corp, Ellicott City, MD 21043 USA.
RI Plaza, Antonio/C-4455-2008; Bernabe Garcia, Sergio/H-5350-2015
OI Plaza, Antonio/0000-0002-9613-1659; Bernabe Garcia,
Sergio/0000-0001-9916-0634
FU Spanish Ministry of Science and Innovation (CEOS-SPAIN project)
[AYA2011-29334-C02-02]; Spanish Ministry of Science and Innovation
FX Manuscript received February 28, 2012; revised October 01, 2012;
accepted February 20, 2013. Date of publication April 18, 2013; date of
current version May 13, 2013. This work was supported by the Spanish
Ministry of Science and Innovation (CEOS-SPAIN project, reference
AYA2011-29334-C02-02).; The authors thank Prof. Melba Crawford from
Purdue University for graciously providing the EO-1 Hyperion data sets,
along with the references signatures and ground-truth used in
experiments. Funding from the Spanish Ministry of Science and Innovation
is also gratefully acknowledged. The authors also thank the editors and
the two anonymous reviewers for their outstanding comments and
suggestions, which greatly helped to improve the technical quality and
presentation of the manuscript.
NR 28
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U1 0
U2 7
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 1939-1404
J9 IEEE J-STARS
JI IEEE J. Sel. Top. Appl. Earth Observ. Remote Sens.
PD APR
PY 2013
VL 6
IS 2
SI SI
BP 408
EP 418
DI 10.1109/JSTARS.2013.2250256
PN 1
PG 11
WC Engineering, Electrical & Electronic; Geography, Physical; Remote
Sensing; Imaging Science & Photographic Technology
SC Engineering; Physical Geography; Remote Sensing; Imaging Science &
Photographic Technology
GA 148VV
UT WOS:000319277100016
ER
PT J
AU Thenkabail, PS
Mariotto, I
Gumma, MK
Middleton, EM
Landis, DR
Huemmrich, KF
AF Thenkabail, Prasad S.
Mariotto, Isabella
Gumma, Murali Krishna
Middleton, Elizabeth M.
Landis, David R.
Huemmrich, K. Fred
TI Selection of Hyperspectral Narrowbands (HNBs) and Composition of
Hyperspectral Twoband Vegetation Indices (HVIs) for Biophysical
Characterization and Discrimination of Crop Types Using Field
Reflectance and Hyperion/EO-1 Data
SO IEEE JOURNAL OF SELECTED TOPICS IN APPLIED EARTH OBSERVATIONS AND REMOTE
SENSING
LA English
DT Article
DE Hyperion; field reflectance; imaging spectroscopy; HyspIRI; biophysical
parameters; hyperspectral vegetation indices; hyperspectral narrowbands;
broadbands
ID WATER PRODUCTIVITY; IRRIGATED WHEAT; ENERGY FLUXES; IMAGERY
AB The overarching goal of this study was to establish optimal hyperspectral vegetation indices (HVIs) and hyperspectral narrowbands (HNBs) that best characterize, classify, model, and map the world's main agricultural crops. The primary objectives were: (1) crop biophysical modeling through HNBs and HVIs, (2) accuracy assessment of crop type discrimination using Wilks' Lambda through a discriminant model, and (3) meta-analysis to select optimal HNBs and HVIs for applications related to agriculture. The study was conducted using two Earth Observing One (EO-1) Hyperion scenes and other surface hyperspectral data for the eight leading worldwide crops (wheat, corn, rice, barley, soybeans, pulses, cotton, and alfalfa) that occupy similar to 70% of all cropland areas globally. This study integrated data collected from multiple study areas in various agroecosystems of Africa, the Middle East, Central Asia, and India. Data were collected for the eight crop types in six distinct growth stages. These included (a) field spectroradiometer measurements (350-2500 nm) sampled at 1-nm discrete bandwidths, and (b) field biophysical variables (e.g., biomass, leaf area index) acquired to correspond with spectroradiometer measurements. The eight crops were described and classified using similar to 20 HNBs. The accuracy of classifying these 8 crops using HNBs was around 95%, which was similar to 25% better than the multi-spectral results possible from Landsat-7's Enhanced Thematic Mapper+ or EO-1's Advanced Land Imager. Further, based on this research and meta-analysis involving over 100 papers, the study established 33 optimal HNBs and an equal number of specific two-band normalized difference HVIs to best model and study specific biophysical and biochemical quantities of major agricultural crops of the world. Redundant bands identified in this study will help overcome the Hughes Phenomenon (or "the curse of high dimensionality") in hyperspectral data for a particular application (e.g., biophysical characterization of crops). The findings of this study will make a significant contribution to future hyperspectral missions such as NASA's HyspIRI.
C1 [Thenkabail, Prasad S.] US Geol Survey, Western Geog Sci Ctr, Flagstaff, AZ 86001 USA.
[Mariotto, Isabella] Univ Texas El Paso, Dept Geol Sci, Environm Sci Program, El Paso, TX 79968 USA.
[Gumma, Murali Krishna] Int Crops Res Inst Semi Arid Trop, South Asia Breeding Hub, IRRI, Patancheru 502324, Andhra Pradesh, India.
[Middleton, Elizabeth M.] NASA, Goddard Space Flight Ctr, Biospher Sci Lab, Greenbelt, MD 20771 USA.
[Landis, David R.] Sigma Space Corp Inc, Lanham, MD 20706 USA.
[Huemmrich, K. Fred] Univ Maryland Baltimore Cty, Baltimore, MD 21228 USA.
RP Thenkabail, PS (reprint author), US Geol Survey, Western Geog Sci Ctr, Flagstaff, AZ 86001 USA.
EM pthenkabail@usgs.gov
FU U.S. Geological Survey; NASA Science Mission Directorate's Earth Science
Division [NNH10ZDA001N-HYSPIRI]; USGS John Wesley Powell Center for
Analysis and Synthesis
FX The authors want to thank Dr. Zhuoting Wu for help with Figs. 3 and 8.
The four anonymous reviewers and two internal USGS reviewers (Dr. Dennis
Dye and Dr. Kristin Byrd) were very insightful in their comments and
helped improve the quality of this manuscript. We are grateful to Dr.
Elizabeth Middleton, NASA, Guest Editor of this special issue, for the
encouragement to put this paper together. Dr. David Landis, Sigma Space
Corp. for editing the penultimate version along with Dr. Middleton. The
financial support through Land Remote Sensing (LRS) and Geographic
Analysis and Monitoring (GAM) Programs of the U.S. Geological Survey are
gratefully acknowledged. The authors are thankful to NASA Science
Mission Directorate's Earth Science Division for the research grant in
response to NASA ROSES HyspIRI solicitation (NNH10ZDA001N-HYSPIRI). The
authors are grateful for continued support and encouragement from Susan
Benjamin, Director of the USGS Western Geographic Science Center and
Edwin Pfeifer, USGS Southwest Geographic Team Chief. Finally, the
authors would like to thank USGS John Wesley Powell Center for Analysis
and Synthesis for funding the Working group on Global Croplands (WGGC).
Our special thanks to Powell Center Directors: Jill Baron and Marty
Goldhaber. Inputs from WGGC team members
(http://powellcenter.usgs.gov/currentprojects.php#GlobalCroplandMembers)
are acknowledged. The WGGC web site
(https://powellcenter.usgs.gov/globalcroplandwater/) support provided by
Megan Eberhardt Frank, Gail A. Montgomery, Tim Kern and others is deeply
appreciated.
NR 43
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U1 3
U2 52
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 1939-1404
J9 IEEE J-STARS
JI IEEE J. Sel. Top. Appl. Earth Observ. Remote Sens.
PD APR
PY 2013
VL 6
IS 2
SI SI
BP 427
EP 439
DI 10.1109/JSTARS.2013.2252601
PN 1
PG 13
WC Engineering, Electrical & Electronic; Geography, Physical; Remote
Sensing; Imaging Science & Photographic Technology
SC Engineering; Physical Geography; Remote Sensing; Imaging Science &
Photographic Technology
GA 148VV
UT WOS:000319277100018
ER
PT J
AU Masi, E
Bellan, J
Harstad, KG
Okong'o, NA
AF Masi, Enrica
Bellan, Josette
Harstad, Kenneth G.
Okong'o, Nora A.
TI Multi-species turbulent mixing under supercritical-pressure conditions:
modelling, direct numerical simulation and analysis revealing species
spinodal decomposition
SO JOURNAL OF FLUID MECHANICS
LA English
DT Article
DE mixing; turbulent mixing
ID MASS DIFFUSION-COEFFICIENTS; SHEAR-LAYER; BINARY; TRANSITION; METHANE;
NUMBER; FLAMES; AIR
AB A model is developed for describing mixing of several species under high-pressure conditions. The model includes the Peng-Robinson equation of state, a full mass-diffusion matrix, a full thermal-diffusion-factor matrix necessary to incorporate the Soret and Dufour effects and both thermal conductivity and viscosity computed for the species mixture using mixing rules. Direct numerical simulations (DNSs) are conducted in a temporal mixing layer configuration. The initial mean flow is perturbed using an analytical perturbation which is consistent with the definition of vorticity and is divergence free. Simulations are performed for a set of five species relevant to hydrocarbon combustion and an ensemble of realizations is created to explore the effect of the initial Reynolds number and of the initial pressure. Each simulation reaches a transitional state having turbulent characteristics and most of the data analysis is performed on that state. A mathematical reformulation of the flux terms in the conservation equations allows the definition of effective species-specific Schmidt numbers (Sc) and of an effective Prandtl number (Pr) based on effective species-specific diffusivities and an effective thermal conductivity, respectively. Because these effective species-specific diffusivities and the effective thermal conductivity are not directly computable from the DNS solution, we develop models for both of these quantities that prove very accurate when compared with the DNS database. For two of the five species, values of the effective species-specific diffusivities are negative at some locations indicating that these species experience spinodal decomposition; we determine the necessary and sufficient condition for spinodal decomposition to occur. We also show that flows displaying spinodal decomposition have enhanced vortical characteristics and trace this aspect to the specific features of high-density-gradient magnitude regions formed in the flows. The largest values of the effective species-specific S c numbers can be well in excess of those known for gases but almost two orders of magnitude smaller than those of liquids at atmospheric pressure. The effective thermal conductivity also exhibits negative values at some locations and the effective Pr displays values that can be as high as those of a liquid refrigerant. Examination of the equivalence ratio indicates that the stoichiometric region is thin and coincides with regions where the mixture effective species-specific Lewis number values are well in excess of unity. Very lean and very rich regions coexist in the vicinity of the stoichiometric region. Analysis of the dissipation indicates that it is dominated by mass diffusion, with viscous dissipation being the smallest among the three dissipation modes. The sum of the heat and species (i.e. scalar) dissipation is functionally modelled using the effective species-specific diffusivities and the effective thermal conductivity. Computations of the modelled sum employing the modelled effective species-specific diffusivities and the modelled effective thermal conductivity shows that it accurately replicates the exact equivalent dissipation.
C1 [Masi, Enrica; Bellan, Josette] CALTECH, Pasadena, CA 91125 USA.
[Bellan, Josette; Harstad, Kenneth G.; Okong'o, Nora A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Bellan, J (reprint author), CALTECH, Pasadena, CA 91125 USA.
EM josette.bellan@jpl.nasa.gov
FU Department of Energy (DOE), Basic Energy Sciences (BES); JPL Research
and Technology Development under the Spontaneous Concepts program under
the DOE-BES
FX This work was conducted at the Jet Propulsion Laboratory (JPL) of the
California Institute of Technology (Caltech) and sponsored by the
Department of Energy (DOE), Basic Energy Sciences (BES) under the
direction of Dr W. Sisk and Dr M. Pederson. Sponsorship from the JPL
Research and Technology Development under the Spontaneous Concepts
program permitted the development of some ideas which were fully
explored under the DOE-BES sponsorship. The computational resources were
provided by the JPL Supercomputing Center, by NASA Advanced
Supercomputing at Ames Research Center and by National Energy Research
Supercomputing Center of the Department of Energy.
NR 39
TC 7
Z9 7
U1 0
U2 25
PU CAMBRIDGE UNIV PRESS
PI NEW YORK
PA 32 AVENUE OF THE AMERICAS, NEW YORK, NY 10013-2473 USA
SN 0022-1120
J9 J FLUID MECH
JI J. Fluid Mech.
PD APR
PY 2013
VL 721
BP 578
EP 626
DI 10.1017/jfm.2013.70
PG 49
WC Mechanics; Physics, Fluids & Plasmas
SC Mechanics; Physics
GA 147IT
UT WOS:000319160800008
ER
PT J
AU Lawrence, SJ
Stopar, JD
Hawke, BR
Greenhagen, BT
Cahill, JTS
Bandfield, JL
Jolliff, BL
Denevi, BW
Robinson, MS
Glotch, TD
Bussey, DBJ
Spudis, PD
Giguere, TA
Garry, WB
AF Lawrence, Samuel J.
Stopar, Julie D.
Hawke, B. Ray
Greenhagen, Benjamin T.
Cahill, Joshua T. S.
Bandfield, Joshua L.
Jolliff, Bradley L.
Denevi, Brett W.
Robinson, Mark S.
Glotch, Timothy D.
Bussey, D. Benjamin J.
Spudis, Paul D.
Giguere, Thomas A.
Garry, W. Brent
TI LRO observations of morphology and surface roughness of volcanic cones
and lobate lava flows in the Marius Hills
SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS
LA English
DT Article
DE Moon; LROC; Diviner; Mini-RF; volcanism; domes; cones; block abundance;
surface roughness; lava flows
ID DIVINER LUNAR RADIOMETER; THERMAL INFRARED-SPECTRA; PLANETARY SURFACES;
CINDER CONES; MOON; EMPLACEMENT; HAWAII; MARS; INSTRUMENT; TRANSITION
AB The volcanic domes, cones, sinuous rilles, and pyroclastic deposits of the Marius Hills region of the Moon (similar to 13.4 degrees N, 304.6 degrees E) represent a significant episode of magmatic activity at or near the lunar surface that is still poorly understood. Comparisons between LROC NAC block populations, Mini-RF data, and Diviner-derived rock abundances confirm that blocky lava flows comprise the domes of the Marius Hills. 8 mu m features measured by Diviner indicate that the domes are not rich in silica and are not significantly different than surrounding mare materials. LROC observations indicate that some of the dome-building lava flows originated directly from volcanic cones. Many of the cones are C-shaped, while others are irregularly shaped, and local topography and lava eruptions affect cone shape. In general, the cones are morphologically similar to terrestrial cinder and lava cones and are composed of varying amounts of cinder, spatter, and lava. Many of the cones are found in local groupings or alignments. The wide range of volcanic features, from broad low domes to steep cones, represents a range of variable eruption conditions. Complex morphologies and variable layering show that eruption conditions were variable over the plateau.
C1 [Lawrence, Samuel J.; Stopar, Julie D.; Robinson, Mark S.] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85287 USA.
[Hawke, B. Ray; Giguere, Thomas A.] Univ Hawaii, Hawaii Inst Geophys & Planetol, Sch Ocean & Earth Sci & Technol, Honolulu, HI 96822 USA.
[Greenhagen, Benjamin T.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Cahill, Joshua T. S.; Denevi, Brett W.; Bussey, D. Benjamin J.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD USA.
[Bandfield, Joshua L.] Univ Washington, Dept Earth & Space Sci, Seattle, WA 98195 USA.
[Jolliff, Bradley L.] Washington Univ, Dept Earth & Planetary Sci, St Louis, MO 63130 USA.
[Glotch, Timothy D.] SUNY Stony Brook, Dept Geosci, Stony Brook, NY 11794 USA.
[Spudis, Paul D.] Univ Space Res Assoc, Lunar & Planetary Inst, Houston, TX USA.
[Giguere, Thomas A.] Intergraph Corp, Kapolei, HI USA.
[Garry, W. Brent] NASA, Goddard Space Flight Ctr, Planetary Geodynam Lab, Greenbelt, MD 20771 USA.
RP Lawrence, SJ (reprint author), Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85287 USA.
EM Samuel.lawrence@asu.edu
RI Garry, Brent/I-5920-2013; Denevi, Brett/I-6502-2012; Cahill,
Joshua/I-3656-2012; Greenhagen, Benjamin/C-3760-2016;
OI Denevi, Brett/0000-0001-7837-6663; Cahill, Joshua/0000-0001-6874-5533;
Stopar, Julie/0000-0003-1578-3688
FU NASA Lunar Reconnaissance Orbiter project
FX The hard work and dedication of the LROC Science Operations Center team
are gratefully acknowledged. This work was funded by the NASA Lunar
Reconnaissance Orbiter project. This work has made use of the NASA/SAO
Astrophysical Data System. This is Lunar and Planetary Institute
contribution 1721 and Hawaii Institute of Geophysics and Planetology
publication 2004.
NR 73
TC 12
Z9 13
U1 1
U2 8
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-9097
EI 2169-9100
J9 J GEOPHYS RES-PLANET
JI J. Geophys. Res.-Planets
PD APR
PY 2013
VL 118
IS 4
BP 615
EP 634
DI 10.1002/jgre.20060
PG 20
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 147GR
UT WOS:000319155000002
ER
PT J
AU Bishop, JL
Perry, KA
Dyar, MD
Bristow, TF
Blake, DF
Brown, AJ
Peel, SE
AF Bishop, Janice L.
Perry, Kaysea A.
Dyar, M. Darby
Bristow, Thomas F.
Blake, David F.
Brown, Adrian J.
Peel, Samantha E.
TI Coordinated spectral and XRD analyses of magnesite-nontronite-forsterite
mixtures and implications for carbonates on Mars
SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS
LA English
DT Article
DE Martian mineralogy; carbonates; reflectance spectroscopy; Mossbauer
spectroscopy; XRD
ID THERMAL EMISSION-SPECTRA; COMMON GEOLOGIC MINERALS; PHOENIX LANDING
SITE; REFLECTANCE SPECTROSCOPY; MOSSBAUER-SPECTROSCOPY; SPECTROMETER
EXPERIMENT; GEOCHEMICAL ANALYSES; SPIRIT ROVER; MARTIAN SOIL;
IDENTIFICATION
AB Mineral detection on Mars largely relies on laboratory data of minerals and mineral mixtures. The objective of this study is to provide reflectance spectra in the visible/near-infrared (VNIR) and mid-IR regions, X-ray diffraction (XRD) data and Mossbauer spectra of a suite of carbonate, phyllosilicate and olivine mixtures in order to facilitate identification and characterization of these minerals on Mars. Remote sensing observations indicate that combinations of these minerals are present in ancient rocks on Mars around the Isidis Basin and in Gusev crater. Magnesite, nontronite, and forsterite size fractions <125 mu m were selected for this study. Results of the VNIR reflectance analyses illustrate the complexity of VNIR spectra of mixtures. Analyses of the NIR band depths near 2.3, 2.5, 3.4, and 4 mu m showed clear trends with carbonate abundance, although the data are not linear. Mixtures of magnesite and nontronite exhibited a band near 2.3 mu m much closer to that observed for nontronite than that for magnesite. VNIR analyses of the mixtures indicated that a small amount of forsterite in any of the mixtures contributed a large increase in the broad similar to 1 mu m band and, hence, the red slope characteristic of Fe2+-bearing minerals. Mid-IR mixture spectra were dominated by magnesite and forsterite, and nontronite was much more difficult to detect by mid-IR spectra in the mixtures. This could be related to why phyllosilicates are detected in many locations on Mars using data collected by the Compact Reconnaissance Imaging Spectrometer for Mars, but not detected using data collected by the Thermal Emission Spectrometer. Mossbauer spectroscopy is well suited for analyses of Fe2+- and Fe3+-bearing minerals, and modeling of the peak areas gave well-correlated trends for nontronite and forsterite abundances where abundant Fe was present. XRD full-pattern fitting analyses were performed on the magnesite-forsterite series, giving results within 6 wt % of the actual values, with a mean difference between actual and calculated values of 2.4 wt %. This study provides important laboratory data for characterizing the spectral and XRD properties of mineral mixtures that will facilitate mineral identification on Mars. Carbonates, in particular, have been primarily observed at low abundances and in small outcrops, and they are frequently found mixed with other minerals. Through analyses of mineral mixtures using multiple data sets, this study seeks to provide ground truthing that will enable better coordination of carbonate detections in the dust and rocks of Mars.
C1 [Bishop, Janice L.; Perry, Kaysea A.; Brown, Adrian J.] SETI Inst, Carl Sagan Ctr, Mountain View, CA 94043 USA.
[Bishop, Janice L.; Bristow, Thomas F.; Blake, David F.; Brown, Adrian J.] NASA Ames Res Ctr, Exobiol Branch, Moffett Field, CA USA.
[Dyar, M. Darby; Peel, Samantha E.] Mt Holyoke Coll, Dept Astron, S Hadley, MA USA.
RP Bishop, JL (reprint author), SETI Inst, Carl Sagan Ctr, Mountain View, CA 94043 USA.
EM jbishop@seti.org
OI Peel, Samantha/0000-0002-2285-6446
FU NASA's MFR; PGG; NASA Postdoctoral Program; National Science Foundation;
NASA Astrobiology Institute
FX The authors thank NASA's MFR and PGG programs and MRO and MSL missions
for partial support of this work. Support from the NASA Postdoctoral
Program to T. Bristow and from the National Science Foundation and the
NASA Astrobiology Institute to K. Perry through the Research Experience
for Undergraduates program at the SETI Institute are greatly
appreciated. Thanks are also due to NASA's PGG program and the NASA
Lunar Science Institute for supporting Brown University's RELAB
facility. Helpful comments from an anonymous reviewer and B. Sutter
improved the manuscript.
NR 94
TC 8
Z9 8
U1 3
U2 33
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-9097
EI 2169-9100
J9 J GEOPHYS RES-PLANET
JI J. Geophys. Res.-Planets
PD APR
PY 2013
VL 118
IS 4
BP 635
EP 650
DI 10.1002/jgre.20066
PG 16
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 147GR
UT WOS:000319155000003
ER
PT J
AU Song, E
Bandfield, JL
Lucey, PG
Greenhagen, BT
Paige, DA
AF Song, Eugenie
Bandfield, Joshua L.
Lucey, Paul G.
Greenhagen, Benjamin T.
Paige, David A.
TI Bulk mineralogy of lunar crater central peaks via thermal infrared
spectra from the Diviner Lunar Radiometer: A study of the Moon's crustal
composition at depth
SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS
LA English
DT Article
DE Lunar crust; Thermal Infrared spectroscopy; Lunar bulk composition
ID PLANETARY SURFACES; EMISSION-SPECTRA; COPERNICUS; CLEMENTINE; OLIVINE;
SOILS; MODEL; SPECTROSCOPY; TOPOGRAPHY; SCATTERING
AB The central peaks of lunar impact craters are thought to be composed of uplifted material originating from varying depths of the crustal column. The interpreted crystallization sequence of the early lunar magma ocean resulted in an anorthositic upper crust that may become progressively more mafic as it approaches the olivine-rich mantle. Emissivity spectra from the Lunar Reconnaissance Orbiter (LRO) Diviner Radiometer are used to derive the wavelength location of the Christiansen Feature (CF), which is sensitive to bulk silicate mineralogy. Here a survey of CF values has been performed for the central peaks of 135 complex craters, providing global and regional observations of the heterogeneity of crustal compositions. Crustal thickness models give context to the preimpact depth of the central peak material and its proximity to the crust-mantle boundary. This study has identified six craters with potentially ultramafic compositions within their central peaks. More common occurrences of mafic material, found in a wide variety of crater central peaks, show a silicate composition roughly similar to mare basalt or an olivine-bearing gabbro. The range of central peak CF values is similar to that of the rest of the lunar surface. Bulk mineralogy of the central peak material does not appear to be correlated with its crustal depth of origin, suggesting both lateral and vertical heterogeneity in crustal composition rather than a gradual transition from felsic to mafic composition. It is likely that the Moon's extensive cratering history has continually overturned the original crust, erasing any original systematic dependence of composition on depth or proximity to the mantle.
C1 [Song, Eugenie; Bandfield, Joshua L.] Univ Washington, Seattle, WA 98195 USA.
[Lucey, Paul G.] Univ Hawaii Manoa, Hawaii Inst Geophys & Planetol, Honolulu, HI 96822 USA.
[Greenhagen, Benjamin T.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Paige, David A.] Univ Calif Los Angeles, Dept Earth & Space Sci, Los Angeles, CA 90024 USA.
RP Song, E (reprint author), Univ Hawaii Manoa, Hawaii Inst Geophys & Planetol, 1680 East West Rd,POST 602, Honolulu, HI 96822 USA.
EM eugesong@higp.hawaii.edu
RI Greenhagen, Benjamin/C-3760-2016
FU operations teams at UCLA; Jet Propulsion Laboratory
FX We would like to thank the Diviner science and operations teams at UCLA
and Jet Propulsion Laboratory for their support. Thanks also to
Jean-Pierre Williams at UCLA for developing data processing scripts that
were vital for this project, Mark Sullivan at UCLA for technical
support. Many thanks to Alan Gillespie and Bruce Nelson at University of
Washington for feedback and advice. Finally, thanks to Joshua T. Cahill
and an anonymous reviewer for their time and constructive advice that
led to the publication of this manuscript.
NR 76
TC 12
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U1 0
U2 8
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0148-0227
J9 J GEOPHYS RES-PLANET
JI J. Geophys. Res.-Planets
PD APR
PY 2013
VL 118
IS 4
BP 689
EP 707
DI 10.1002/jgre.20065
PG 19
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 147GR
UT WOS:000319155000006
ER
PT J
AU Datta, A
Yeo, H
Norman, TR
AF Datta, Anubhav
Yeo, Hyeonsoo
Norman, Thomas R.
TI Experimental Investigation and Fundamental Understanding of a Full-Scale
Slowed Rotor at High Advance Ratios
SO JOURNAL OF THE AMERICAN HELICOPTER SOCIETY
LA English
DT Article
ID COMPOUND HELICOPTER; TECHNOLOGY
AB This paper describes and analyzes the measurements from a full-scale, slowed revolutions per minute (rpm), UH-60A rotor tested at the National Full-Scale Aerodynamics Complex 40- by 80-ft wind tunnel up to an advance ratio of 1.0. A comprehensive set of measurements that includes performance, blade loads, hub loads, and pressures/airloads makes this data set unique. The measurements reveal new and rich aeromechanical phenomena that are unique to this exotic regime. These include reverse chord dynamic stall, retreating side impulse in torsion load, large inboard outboard elastic twist differential, diminishing rotor forces and yet a dramatic buildup of blade loads, and high blade loads and yet benign levels of vibratory hub loads. The objective of this research is the fundamental understanding of these unique aeromechanical phenomena. The intent is to provide useful knowledge for the design of high-speed, high-efficiency, slowed rpm rotors of the future and a database for validation of advanced analyses.
C1 [Datta, Anubhav] NASA, Ames Res Ctr, Sci & Technol Corp, USA,Aeroflightdynam Directorate, Moffett Field, CA 94035 USA.
[Yeo, Hyeonsoo] NASA, Ames Res Ctr, Aeroflightdynam Directorate AMRDEC, USA,Res Dev & Engn Command, Moffett Field, CA 94035 USA.
[Norman, Thomas R.] NASA, Ames Res Ctr, Aeromech Branch, Moffett Field, CA 94035 USA.
RP Datta, A (reprint author), NASA, Ames Res Ctr, Sci & Technol Corp, USA,Aeroflightdynam Directorate, Moffett Field, CA 94035 USA.
EM hubloads@gmail.com
NR 39
TC 10
Z9 10
U1 0
U2 7
PU AMER HELICOPTER SOC INC
PI ALEXANDRIA
PA 217 N WASHINGTON ST, ALEXANDRIA, VA 22314 USA
SN 0002-8711
J9 J AM HELICOPTER SOC
JI J. Am. Helicopter Soc.
PD APR
PY 2013
VL 58
IS 2
AR 022004
DI 10.4050/JAHS.58.022004
PG 17
WC Engineering, Aerospace
SC Engineering
GA 147NF
UT WOS:000319173600004
ER
PT J
AU Yeo, H
Romander, EA
AF Yeo, Hyeonsoo
Romander, Ethan A.
TI Loads Correlation of a Full-Scale UH-60A Air loads Rotor in a Wind
Tunnel
SO JOURNAL OF THE AMERICAN HELICOPTER SOCIETY
LA English
DT Article
ID COMPREHENSIVE ANALYSIS; HELICOPTER ROTORS; AIRLOADS; PERFORMANCE;
PREDICTION; SYSTEM
AB Wind tunnel measurements of the rotor trim, blade airloads, and structural loads of a full-scale UH-60A Black Hawk main rotor are compared with calculations obtained using the comprehensive rotorcraft analysis CAMRAD II and a coupled CAMRAD II/OVERFLOW 2 analysis. A speed sweep at constant lift up to an advance ratio of 0.4 and a thrust sweep at constant speed into deep stall are investigated. The coupled analysis shows significant improvement over comprehensive analysis. Normal force phase is better captured for all the test conditions examined. Pitching moment is better predicted, including the magnitude and phase of the two stall events in the fourth quadrant at the deeply stalled condition. Structural loads are, in general, improved with the coupled analysis, but the magnitude of chord bending moment is still significantly underpredicted. As there are three modes around 4 and 5/rev frequencies, the structural responses to the 5/rev airloads due to dynamic stall are magnified and thus accurate analysis of the deeply stalled condition is challenging.
C1 [Yeo, Hyeonsoo] NASA, Ames Res Ctr, Aeroflightdynam Directorate AMRDEC, USA,Res Dev & Engn Command, Moffett Field, CA 94035 USA.
[Romander, Ethan A.] NASA, Ames Res Ctr, Flight Vehicle Res & Technol Div, Moffett Field, CA 94035 USA.
RP Yeo, H (reprint author), NASA, Ames Res Ctr, Aeroflightdynam Directorate AMRDEC, USA,Res Dev & Engn Command, Moffett Field, CA 94035 USA.
EM hyeonsoo.yeo.civ@mail.mil
NR 20
TC 1
Z9 1
U1 0
U2 3
PU AMER HELICOPTER SOC INC
PI ALEXANDRIA
PA 217 N WASHINGTON ST, ALEXANDRIA, VA 22314 USA
SN 0002-8711
J9 J AM HELICOPTER SOC
JI J. Am. Helicopter Soc.
PD APR
PY 2013
VL 58
IS 2
DI 10.4050/JAHS.58.022003
PG 18
WC Engineering, Aerospace
SC Engineering
GA 147NF
UT WOS:000319173600003
ER
PT J
AU Dauser, T
Garcia, J
Wilms, J
Bock, M
Brenneman, LW
Falanga, M
Fukumura, K
Reynolds, CS
AF Dauser, T.
Garcia, J.
Wilms, J.
Boeck, M.
Brenneman, L. W.
Falanga, M.
Fukumura, K.
Reynolds, C. S.
TI Irradiation of an accretion disc by a jet: general properties and
implications for spin measurements of black holes
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE accretion, accretion discs; black hole physics; lines: profiles;
galaxies: active; galaxies: nuclei
ID X-RAY REFLECTION; ADVECTION-DOMINATED ACCRETION; K-ALPHA LINE;
XMM-NEWTON; IRON LINE; CYGNUS X-1; GX 339-4; ACTIVE GALAXY; 1H 0707-495;
HARD STATE
AB X-ray irradiation of the accretion disc leads to strong reflection features, which are then broadened and distorted by relativistic effects. We present a detailed, general relativistic approach to model this irradiation for different geometries of the primary X-ray source. These geometries include the standard point source on the rotational axis as well as more jet-like sources, which are radially elongated and accelerating. Incorporating this code in the RELLINE model for relativistic line emission, the line shape for any configuration can be predicted. We study how different irradiation geometries affect the determination of the spin of the black hole. Broad emission lines are produced only for compact irradiating sources situated close to the black hole. This is the only case where the black hole spin can be unambiguously determined. In all other cases the line shape is narrower, which could either be explained by a low spin or an elongated source. We conclude that in those cases and independent of the quality of the data no unique solution for the spin exists and therefore only a lower limit of the spin value can be given.
C1 [Dauser, T.; Wilms, J.; Boeck, M.] Dr Karl Remeis Observ, D-96049 Bamberg, Germany.
[Dauser, T.; Wilms, J.; Boeck, M.] Erlangen Ctr Astroparticle Phys, D-96049 Bamberg, Germany.
[Garcia, J.; Reynolds, C. S.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Garcia, J.; Reynolds, C. S.] Univ Maryland, Maryland Astron Ctr Theory & Computat, College Pk, MD 20742 USA.
[Boeck, M.] Max Planck Inst Radioastron, D-53121 Bonn, Germany.
[Brenneman, L. W.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Falanga, M.] Int Space Sci Inst, CH-3012 Bern, Switzerland.
[Fukumura, K.] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA.
RP Dauser, T (reprint author), Dr Karl Remeis Observ, Sternwartstr 7, D-96049 Bamberg, Germany.
EM thomas.dauser@sternwarte.uni-erlangen.de
RI Wilms, Joern/C-8116-2013
OI Wilms, Joern/0000-0003-2065-5410
FU European Commission [ITN 215212]; Elitenetzwerk Bayern; Deutsches
Zentrum fur Luft- und Raumfahrt [50 OR 1113]
FX We acknowledge support from the European Commission under contract ITN
215212 'Black Hole Universe' by a fellowship from the Elitenetzwerk
Bayern, and by the Deutsches Zentrum fur Luft- und Raumfahrt under
contract number 50 OR 1113. We thank John E. Davis for the development
of the SLXFIG module used to prepare the figures in this paper, Katja
Pottschmidt and John Tomsick for useful discussions, and the referee,
Andy Fabian, for his constructive comments which helped in improving
this paper.
NR 105
TC 68
Z9 68
U1 0
U2 2
PU OXFORD UNIV PRESS
PI OXFORD
PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND
SN 0035-8711
EI 1365-2966
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD APR
PY 2013
VL 430
IS 3
BP 1694
EP 1708
DI 10.1093/mnras/sts710
PG 15
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 148QG
UT WOS:000319260500014
ER
PT J
AU Szabados, L
Derekas, A
Kiss, LL
Kovacs, J
Anderson, RI
Kiss, C
Szalai, T
Szekely, P
Christiansen, JL
AF Szabados, L.
Derekas, A.
Kiss, L. L.
Kovacs, J.
Anderson, R. I.
Kiss, Cs.
Szalai, T.
Szekely, P.
Christiansen, J. L.
TI Discovery of the spectroscopic binary nature of six southern Cepheids
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE binaries: spectroscopic; stars: variables: Cepheids
ID RADIAL-VELOCITIES; VARIABLE-STARS; INTERMEDIATE-BAND; PERIOD CEPHEIDS;
HEMISPHERE; SPECTROGRAPH; PHOTOMETRY
AB We present the analysis of photometric and spectroscopic data of six bright Galactic Cepheids: GH Carinae, V419 Centauri, V898 Centauri, AD Puppis, AY Sagittarii and ST Velorum. Based on new radial velocity data (in some cases supplemented with earlier data available in the literature), these Cepheids have been found to be members in spectroscopic binary systems. V898 Cen turned out to have one of the largest orbital radial velocity amplitude (>40 km s(-1)) among the known binary Cepheids. The data are insufficient to determine the orbital periods nor other orbital elements for these new spectroscopic binaries.
These discoveries corroborate the statement on the high frequency of occurrence of binaries among the classical Cepheids, a fact to be taken into account when calibrating the period-luminosity relationship for Cepheids.
We have also compiled all available photometric data that revealed that the pulsation period of AD Pup, the longest period Cepheid in this sample, is continuously increasing with Delta P = 0.004567d century(-1), likely to be caused by stellar evolution. The wave-like pattern superimposed on the parabolic O - C graph of AD Pup may well be caused by the light-time effect in the binary system. ST Vel also pulsates with a continuously increasing period. The other four Cepheids are characterized with stable pulsation periods in the last half century.
C1 [Szabados, L.; Derekas, A.; Kiss, L. L.; Kiss, Cs.] Hungarian Acad Sci, Res Ctr Astron & Earth Sci, Konkoly Observ, H-1121 Budapest, Hungary.
[Derekas, A.; Kiss, L. L.] Univ Sydney, Sch Phys, Sydney Inst Astron, Sydney, NSW 2006, Australia.
[Kiss, L. L.; Kovacs, J.] ELTE Gothard Lendulet Res Grp, H-9700 Szombathely, Hungary.
[Anderson, R. I.] Univ Geneva, Observ Geneve, CH-1290 Versoix, Switzerland.
[Szalai, T.] Univ Szeged, Dept Opt & Quantum Elect, H-6720 Szeged, Hungary.
[Szekely, P.] Univ Szeged, Dept Expt Phys, H-6720 Szeged, Hungary.
[Christiansen, J. L.] NASA, Ames Res Ctr, SETI Inst, Moffett Field, CA 94035 USA.
RP Szabados, L (reprint author), Hungarian Acad Sci, Res Ctr Astron & Earth Sci, Konkoly Observ, Konkoly Thege Miklos Ul 15-17, H-1121 Budapest, Hungary.
EM szabados@konkoly.hu
RI Derekas, Aliz/G-2091-2016;
OI Derekas, Aliz/0000-0002-6526-9444; Anderson, Richard
I./0000-0001-8089-4419
FU ESA PECS Project [C98090]; ESTEC [4000106398/12/NL/KML]; Hungarian OTKA
[K76816, K83790, K104607, MB08C 81013]; European Community [269194];
Hungarian Academy of Sciences; Hungarian Eotvos fellowship; Janos Bolyai
Research Scholarship of the Hungarian Academy of Sciences; European
Research Council under the European Community/ERC [227224]
FX This project has been supported by the ESA PECS Project C98090, ESTEC
Contract No. 4000106398/12/NL/KML, the Hungarian OTKA Grants K76816,
K83790, K104607 and MB08C 81013, as well as the European Community's
Seventh Framework Programme (FP7/2007-2013) under grant agreement no.
269194 and the 'Lendulet-2009' Young Researchers Programme of the
Hungarian Academy of Sciences. AD was supported by the Hungarian Eotvos
fellowship. AD has been supported by the Janos Bolyai Research
Scholarship of the Hungarian Academy of Sciences. AD is very thankful to
the staff at The Lodge in Siding Spring Observatory for their
hospitality and the very nice food, making the time spent there lovely
and special. Part of the research leading to these results has received
funding from the European Research Council under the European
Community's Seventh Framework Programme (FP7/2007-2013)/ERC grant
agreement no. 227224 (PROSPERITY). The INTEGRAL photometric data,
pre-processed by ISDC, have been retrieved from the OMC Archive at CAB
(INTA-CSIC). Critical remarks by Dr. Maria Kun and the referee's
suggestions led to a considerable improvement in the presentation of the
results.
NR 46
TC 3
Z9 3
U1 0
U2 2
PU OXFORD UNIV PRESS
PI OXFORD
PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND
SN 0035-8711
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD APR
PY 2013
VL 430
IS 3
BP 2018
EP 2028
DI 10.1093/mnras/stt027
PG 11
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 148QG
UT WOS:000319260500040
ER
PT J
AU Corsaro, E
Frohlich, HE
Bonanno, A
Huber, D
Bedding, TR
Benomar, O
De Ridder, J
Stello, D
AF Corsaro, E.
Froehlich, H. -E.
Bonanno, A.
Huber, D.
Bedding, T. R.
Benomar, O.
De Ridder, J.
Stello, D.
TI A Bayesian approach to scaling relations for amplitudes of solar-like
oscillations in Kepler stars
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE methods: data analysis; methods: statistical; stars: evolution; stars:
late-type; stars: oscillations
ID RED GIANT BRANCH; STELLAR OSCILLATIONS; MAIN-SEQUENCE; OPEN CLUSTERS;
INITIAL CHARACTERISTICS; INPUT CATALOG; CADENCE DATA; HR DIAGRAM; NGC
6819; ASTEROSEISMOLOGY
AB We investigate different amplitude scaling relations adopted for the asteroseismology of stars that show solar-like oscillations. Amplitudes are among the most challenging asteroseismic quantities to handle because of the large uncertainties that arise in measuring the background level in the star's power spectrum. We present results computed by means of a Bayesian inference on a sample of 1640 stars observed with Kepler, spanning from main sequence to red giant stars, for 12 models used for amplitude predictions and exploiting recently well-calibrated effective temperatures from Sloan Digital Sky Survey photometry. We test the candidate amplitude scaling relations by means of a Bayesian model comparison. We find the model having a separate dependence upon the mass of the stars to be largely the most favoured one. The differences among models and the differences seen in their free parameters from early to late phases of stellar evolution are also highlighted.
C1 [Corsaro, E.] Univ Catania, Dept Phys & Astron, Astrophys Sect, I-95123 Catania, Italy.
[Corsaro, E.; Bonanno, A.] INAF Astrophys Observ Catania, I-95123 Catania, Italy.
[Corsaro, E.; De Ridder, J.] Katholieke Univ Leuven, Inst Sterrenkunde, B-3001 Louvain, Belgium.
[Froehlich, H. -E.] Leibniz Inst Astrophys Potsdam AIP, D-14482 Potsdam, Germany.
[Huber, D.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Bedding, T. R.; Benomar, O.; Stello, D.] Univ Sydney, Sch Phys, Sydney Inst Astron SIfA, Sydney, NSW 2006, Australia.
[Bedding, T. R.; Benomar, O.; Stello, D.] Aarhus Univ, Stellar Astrophys Ctr, Dept Phys & Astron, DK-8000 Aarhus C, Denmark.
RP Corsaro, E (reprint author), Univ Catania, Dept Phys & Astron, Astrophys Sect, Via S Sofia 78, I-95123 Catania, Italy.
EM eco@oact.inaf.it
OI Bedding, Timothy/0000-0001-5943-1460; Bonanno,
Alfio/0000-0003-3175-9776; Bedding, Tim/0000-0001-5222-4661
FU PRIN-INAF; FWO-Flanders [O6260 - G.0728.11]; Danish National Research
Foundation; ASTERISK project (ASTERoseismic Investigations with SONG and
Kepler); European Research Council [267864]
FX EC acknowledges financial support from the PRIN-INAF 2010
Asteroseismology: looking inside the stars with space-and ground-based
observations. EC and JDR acknowledge the support of the FWO-Flanders
under project O6260 - G.0728.11. Funding for the Stellar Astrophysics
Centre is provided by the Danish National Research Foundation. The
research is supported by the ASTERISK project (ASTERoseismic
Investigations with SONG and Kepler) funded by the European Research
Council (Grant agreement no.: 267864).
NR 67
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Z9 20
U1 0
U2 1
PU OXFORD UNIV PRESS
PI OXFORD
PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND
SN 0035-8711
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD APR
PY 2013
VL 430
IS 3
BP 2313
EP 2326
DI 10.1093/mnras/stt059
PG 14
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 148QG
UT WOS:000319260500061
ER
PT J
AU Gudipati, MS
Jacovi, R
Couturier-Tamburelli, I
Lignell, A
Allen, M
AF Gudipati, Murthy S.
Jacovi, Ronen
Couturier-Tamburelli, Isabelle
Lignell, Antti
Allen, Mark
TI Photochemical activity of Titan's low-altitude condensed haze
SO NATURE COMMUNICATIONS
LA English
DT Article
ID FAR-INFRARED SPECTRA; HUYGENS LANDING SITE; COUPLING PHOTOCHEMISTRY;
ELECTRONIC-SPECTRUM; EXCITED-STATES; ATMOSPHERE; DICYANOACETYLENE;
AEROSOLS; C4N2; STRATOSPHERE
AB Titan, the largest moon of Saturn and similar to Earth in many aspects, has unique orange-yellow colour that comes from its atmospheric haze, whose formation and dynamics are far from well understood. Present models assume that Titan's tholin-like haze formation occurs high in atmosphere through gas-phase chemical reactions initiated by high-energy solar radiation. Here we address an important question: Is the lower atmosphere of Titan photochemically active or inert? We demonstrate that indeed tholin-like haze formation could occur on condensed aerosols throughout the atmospheric column of Titan. Detected in Titan's atmosphere, dicyanoacetylene (C4N2) is used in our laboratory simulations as a model system for other larger unsaturated condensing compounds. We show that C4N2 ices undergo condensed-phase photopolymerization (tholin formation) at wavelengths as long as 355 nm pertinent to solar radiation reaching a large portion of Titan's atmosphere, almost close to the surface.
C1 [Gudipati, Murthy S.; Jacovi, Ronen; Lignell, Antti; Allen, Mark] CALTECH, Jet Prop Lab, Div Sci, Pasadena, CA 91109 USA.
[Gudipati, Murthy S.] Univ Maryland, IPST, College Pk, MD 20742 USA.
[Couturier-Tamburelli, Isabelle] Aix Marseille Univ, UMR CNRS 7345, Lab Phys Interact Ion & Mol, F-13397 Marseille 20, France.
[Allen, Mark] CALTECH, Dept Geol & Planetary Sci, Pasadena, CA 91125 USA.
RP Gudipati, MS (reprint author), CALTECH, Jet Prop Lab, Div Sci, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM murthy.gudipati@jpl.nasa.gov
RI Gudipati, Murthy/F-7575-2011; Lignell, Antti/C-2146-2009
OI Lignell, Antti/0000-0001-7664-5583
FU NASA Astrobiology Institute team 'Titan as a Prebiotic Chemical System';
Jet Propulsion Laboratory; JPL; Titan organic aerosol spectroscopy and
chemistry (TOAST) laboratory at JPL; French national program
Environnements Planetaires et Origines de la Vie (EPOV)
FX The Jet Propulsion Laboratory (JPL) part of the work is partly supported
by several of the following funding sources: NASA Astrobiology Institute
team 'Titan as a Prebiotic Chemical System', the Jet Propulsion
Laboratory Director's Research and Development Fund and the JPL Research
and Technology Development funding for the infrastructure of the Ice
Spectroscopy Laboratory (ISL) and Titan organic aerosol spectroscopy and
chemistry (TOAST) laboratory at JPL. The University of Provence part of
the work was funded by the French national program Environnements
Planetaires et Origines de la Vie (EPOV). This research was carried out
at the Jet Propulsion Laboratory, California Institute of Technology,
under a contract with the National Aeronautics and Space Administration.
NR 50
TC 10
Z9 10
U1 2
U2 57
PU NATURE PUBLISHING GROUP
PI LONDON
PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND
SN 2041-1723
J9 NAT COMMUN
JI Nat. Commun.
PD APR
PY 2013
VL 4
AR 1648
DI 10.1038/ncomms2649
PG 8
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 143MR
UT WOS:000318872100005
PM 23552063
ER
PT J
AU Rios, J
AF Rios, Joseph
TI Algorithm 928: A General, Parallel Implementation of Dantzig-Wolfe
Decomposition
SO ACM TRANSACTIONS ON MATHEMATICAL SOFTWARE
LA English
DT Article
DE Algorithms; Linear programming; optimization; parallel implementations
ID MATRICES; PROGRAMS
AB Dantzig-Wolfe Decomposition is recognized as a powerful, algorithmic tool for solving linear programs of block-angular form. While use of the approach has been reported in a wide variety of domains, there has not been a general implementation of Dantzig-Wolfe decomposition available. This article describes an open-source implementation of the algorithm. It is general in the sense that any properly decomposed linear program can be provided to the software for solving. While the original description of the algorithm was motivated by its reduced memory usage, modern computers can also take advantage of the algorithm's inherent parallelism. This implementation is parallel and built upon the POSIX threads (pthreads) library. Some computational results are provided to motivate use of such parallel solvers, as this implementation outperforms state-of-the-art commercial solvers in terms of wall-clock runtime by an order of magnitude or more on several problem instances.
C1 [Rios, Joseph] NASA, Moffett Field, CA 94035 USA.
RP Rios, J (reprint author), NASA, Ames Res Ctr, Mail Stop 210-15, Moffett Field, CA 94035 USA.
EM joseph.l.rios@nasa.gov
NR 22
TC 0
Z9 0
U1 0
U2 2
PU ASSOC COMPUTING MACHINERY
PI NEW YORK
PA 2 PENN PLAZA, STE 701, NEW YORK, NY 10121-0701 USA
SN 0098-3500
J9 ACM T MATH SOFTWARE
JI ACM Trans. Math. Softw.
PD APR
PY 2013
VL 39
IS 3
AR 21
DI 10.1145/2450153.2450159
PG 10
WC Computer Science, Software Engineering; Mathematics, Applied
SC Computer Science; Mathematics
GA 140BI
UT WOS:000318628800006
ER
PT J
AU Som, SM
Hagadorn, JW
Thelen, WA
Gillespie, AR
Catling, DC
Buick, R
AF Som, Sanjoy M.
Hagadorn, James W.
Thelen, Weston A.
Gillespie, Alan R.
Catling, David C.
Buick, Roger
TI Quantitative discrimination between geological materials with variable
density contrast by high resolution X-ray computed tomography: An
example using amygdule size-distribution in ancient lava flows
SO COMPUTERS & GEOSCIENCES
LA English
DT Article
DE X-ray tomography; Amygdules; Bubble-size distribution; Dynamic
thresholding; Bootstrap resampling; Central limit theorem
ID BASALT FLOWS; BUBBLE; ROCKS; MICROTOMOGRAPHY; COALESCENCE; ERUPTION
AB The bubble-size distribution in 2.7 billion year old lava flows can be used as a proof of concept illustrating a new set of techniques for measuring volumes of geological materials with variable density contrasts using high-resolution X-ray computed tomography. Such studies have been limited in the past to high-contrast situations such as vesicles devoid of secondary fill. We present a new dynamic thresholding method for computationally separating amygdules from their basaltic matrix in X-ray images that is based on a technique used in seismology. The technique is sensitive to the gradient of the gray-scale value, rather than an absolute threshold value often applied to an entire set of X-ray images. Additionally, we present statistical methods for extrapolating the volumetric measurement mean and standard deviation of amygdules in the measured samples to the entire population in the flow. To do so, we create additional amygdule sample sets from the original sample set in the process of 'bootstrap' resampling, and use the Central Limit Theorem to calculate the mean and standard deviation of the amygdule population from these sample sets. This suite of methods allows the extension of bubble-size distribution studies typically done on modern flows to the ancient rock record and potentially has many other uses in geosciences where quantitative discrimination between materials with a range of densities is required. (C) 2012 Elsevier Ltd. All rights reserved.
C1 [Som, Sanjoy M.; Thelen, Weston A.; Gillespie, Alan R.; Catling, David C.; Buick, Roger] Univ Washington, Dept Earth & Space Sci, Seattle, WA 98195 USA.
[Som, Sanjoy M.] Blue Marble Space Inst Sci, Seattle, WA 98145 USA.
[Hagadorn, James W.] Denver Museum Nat & Sci, Dept Earth Sci, Denver, CO 80205 USA.
[Thelen, Weston A.] Hawaii Volcano Observ, Volcano, HI 96718 USA.
RP Som, SM (reprint author), NASA, Ames Res Ctr, Exobiol Branch, Moffett Field, CA 94035 USA.
EM sanjoy@uw.edu
OI Catling, David/0000-0001-5646-120X; Buick, Roger/0000-0003-0139-1659
FU NASA Exobiology/Astrobiology grant [NNX08AP56G]
FX This work was funded by NASA Exobiology/Astrobiology grant NNX08AP56G.
The help of John Perreault is gratefully acknowledged in assisting with
BLOB3D amygdule extraction. Richard Ketcham and Philip Watson at the UT
HRXCT facility are thanked for their helpful feedback during our
implementation of BLOB3D. This manuscript benefited from constructive
reviews by Richard Ketcham and Guilherme Gualda.
NR 28
TC 3
Z9 3
U1 2
U2 12
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0098-3004
J9 COMPUT GEOSCI-UK
JI Comput. Geosci.
PD APR
PY 2013
VL 54
BP 231
EP 238
DI 10.1016/j.cageo.2012.11.019
PG 8
WC Computer Science, Interdisciplinary Applications; Geosciences,
Multidisciplinary
SC Computer Science; Geology
GA 136PW
UT WOS:000318376900027
ER
PT J
AU Ishikawa, ST
Gulick, VC
AF Ishikawa, Sascha T.
Gulick, Virginia C.
TI An automated mineral classifier using Raman spectra
SO COMPUTERS & GEOSCIENCES
LA English
DT Article
DE Mineral classification; Raman spectroscopy; Machine learning; Mars;
Robotic exploration; Igneous rocks
ID PRINCIPAL COMPONENT ANALYSIS; SPECTROSCOPY; IDENTIFICATION
AB We present a robust and autonomous mineral classifier for analyzing igneous rocks. Our study shows that machine learning methods, specifically artificial neural networks, can be trained using spectral data acquired by in situ Raman spectroscopy in order to accurately distinguish among key minerals for characterizing the composition of igneous rocks. These minerals include olivine, quartz, plagioclase, potassium feldspar, mica, and several pyroxenes. On average, our classifier performed with 83 percent accuracy. Quartz and olivine, as well as the pyroxenes, were classified with 100 percent accuracy. In addition to using traditional features such as the location of spectral bands and their shapes, our automated mineral, classifier was able to incorporate fluorescence patterns, which are not as easily perceived by humans, into its classification scheme. The latter was able to improve the classification accuracy and is an example of the robustness of our classifier. (C) 2013 Elsevier Ltd. All rights reserved.
C1 [Ishikawa, Sascha T.; Gulick, Virginia C.] NASA, Ames Res Ctr, Div Space Sci, Moffett Field, CA 94035 USA.
[Ishikawa, Sascha T.] Univ Calif Santa Cruz, Santa Cruz, CA 95064 USA.
[Gulick, Virginia C.] SETI Inst, Mountain View, CA 94043 USA.
RP Ishikawa, ST (reprint author), NASA, Ames Res Ctr, Div Space Sci, Mail Stop 239-20, Moffett Field, CA 94035 USA.
EM Sascha.T.Ishikawa@nasa.gov
FU NASA
FX We thank Shawn Hart for acquiring the Raman spectra of our samples. This
research was supported by a prior grant from NASA's Advanced Cross
Enterprise Technology Development Program.
NR 26
TC 11
Z9 12
U1 4
U2 23
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0098-3004
J9 COMPUT GEOSCI-UK
JI Comput. Geosci.
PD APR
PY 2013
VL 54
BP 259
EP 268
DI 10.1016/j.cageo.2013.01.011
PG 10
WC Computer Science, Interdisciplinary Applications; Geosciences,
Multidisciplinary
SC Computer Science; Geology
GA 136PW
UT WOS:000318376900030
ER
PT J
AU Won, J
Said, MA
Seyam, AFM
AF Won, Jessica
Said, Magdi A.
Seyam, Abdel-Fattah M.
TI Development of UV Protective Sheath for High Performance Fibers for High
Altitude Applications
SO FIBERS AND POLYMERS
LA English
DT Article
DE High performance fibers; Ultraviolet and visible light; Low density
polyethylene; Zylon (R)
AB High performance fibers have distinguished properties such as high tensile strength, good thermal and chemical resistance, dimensional stability, lightweight, and high electrical conductivity. Due to these superior properties, high performance fibers made it to the scene of broad range of applications such as aerospace, automotive, windmill, fiber reinforced composites, high strength tethers, tendons for scientific balloon, tension structures, protective clothing, and marine. Examples of such fibers are Zylon (R), Kevlar (R), and Vectran (R). However, the fibers lose their strength significantly upon exposure to Ultraviolet (UV) and visible light. In this research, UV protective films from extruded low density polyethylene (LDPE) loaded with different content of UV stabilizers (TiO2 nanoparticles and White PE CC (R)) were investigated. To assess the degree of UV blockage of each extruded protective film, their transmittance to UV and visible (UV-VIS) light was measured. Additionally, Zylon (R) braids were sheathed with the protective films and the strength of the braids and yarns raveled from braids was measured before and after UV exposure for different number of days. LDPE loaded with White PE CC (R) and 10 % TiO2 showed the least transmittance to UV-VIS and their yarns and braids exhibited highest strength retention after exposure to artificial UV. Strength retention of braids was higher than that of individual yarns due to weak link effect and braid structure assistant.
C1 [Won, Jessica] Hyosung Corp, Anyang 431080, South Korea.
[Said, Magdi A.] NASA, Wallops Isl, VA USA.
[Seyam, Abdel-Fattah M.] NC State Univ, Coll Text, Raleigh, NC USA.
RP Seyam, AFM (reprint author), NC State Univ, Coll Text, Raleigh, NC USA.
EM aseyam@ncsu.edu
FU NASA Balloon Program Office [NNXlOAE26G]; State of North Carolina
FX This work is funded by NASA Balloon Program Office (Grant Number
NNXlOAE26G) and the State of North Carolina. The authors extend their
appreciation to Dr. Rahul Vallabh of NC State University College of
Textiles for his valuable discussion.
NR 11
TC 5
Z9 5
U1 2
U2 37
PU KOREAN FIBER SOC
PI SEOUL
PA KOREA SCIENCE TECHNOLOGY CTR #501 635-4 YEOGSAM-DONG, KANGNAM-GU, SEOUL
135-703, SOUTH KOREA
SN 1229-9197
J9 FIBER POLYM
JI Fiber. Polym.
PD APR
PY 2013
VL 14
IS 4
BP 647
EP 652
DI 10.1007/s12221-013-0647-9
PG 6
WC Materials Science, Textiles; Polymer Science
SC Materials Science; Polymer Science
GA 141RA
UT WOS:000318743000020
ER
PT J
AU Reinhart, RC
Kacpura, TJ
Johnson, SK
Lux, JP
AF Reinhart, Richard C.
Kacpura, Thomas J.
Johnson, Sandra K.
Lux, James P.
TI NASA's Space Communications and Navigation Test Bed aboard the
International Space Station
SO IEEE AEROSPACE AND ELECTRONIC SYSTEMS MAGAZINE
LA English
DT Article
C1 [Reinhart, Richard C.; Kacpura, Thomas J.; Johnson, Sandra K.] NASA, John H Glenn Res Ctr, Cleveland, OH 44135 USA.
[Lux, James P.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Reinhart, RC (reprint author), NASA, John H Glenn Res Ctr, 21000 Brookpark Rd,Mail Stop 54-1, Cleveland, OH 44135 USA.
EM richard.c.reinhart@nasa.gov
NR 6
TC 2
Z9 3
U1 0
U2 6
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 0885-8985
J9 IEEE AERO EL SYS MAG
JI IEEE Aerosp. Electron. Syst. Mag.
PD APR
PY 2013
VL 28
IS 4
BP 4
EP 15
PG 12
WC Engineering, Aerospace; Engineering, Electrical & Electronic
SC Engineering
GA 138YF
UT WOS:000318547100002
ER
PT J
AU Mayer, JM
Graves, JE
Manini, TM
Nuzzo, JL
Ploutz-Snyder, LL
AF Mayer, John M.
Graves, James E.
Manini, Todd M.
Nuzzo, James L.
Ploutz-Snyder, Lori L.
TI Lumbar Muscle Activity During Common Lifts: A Preliminary Study Using
Magnetic Resonance Imaging
SO JOURNAL OF APPLIED BIOMECHANICS
LA English
DT Article
DE biomechanics; exercise; MRI; muscle; spine
ID LOW-BACK-PAIN; EXERCISE INTENSITY; RELAXATION-TIMES; SKELETAL-MUSCLE;
WORK; ELECTROMYOGRAPHY; MANAGEMENT; IMAGES; T2
AB The purpose of this preliminary study was to assess lumbar multifidus, erector spinae, and quadratus lumborum muscle activity during lifts as measured by changes in transverse relaxation time (T2) from magnetic resonance imaging (MRI). Thirteen healthy adults performed dynamic squat, stoop, and asymmetric stoop lifts at a standard load, with each lift followed by MRI. Increase in T2 for the multifidus and erector spinae was greater for the stoop than squat. No difference in T2 increase was noted between the multifidus and erector spinae for the squat or stoop. Increase in T2 for the contralateral multifidus was less for the asymmetric stoop than stoop. Future research using MRI and other biomechanical techniques is needed to fully characterize lumbar muscle activity during lifts for various populations, settings, postures, and loads.
C1 [Mayer, John M.; Nuzzo, James L.] Univ S Florida, Coll Med, Sch Phys Therapy & Rehabil Sci, Tampa, FL 33620 USA.
[Graves, James E.] Univ Utah, Coll Hlth, Salt Lake City, UT USA.
[Manini, Todd M.] Univ Florida, Coll Med, Dept Aging & Geriatr Res, Gainesville, FL USA.
[Ploutz-Snyder, Lori L.] NASA Johnson Space Ctr, Univ Space Res Assoc, Houston, TX USA.
RP Mayer, JM (reprint author), Univ S Florida, Coll Med, Sch Phys Therapy & Rehabil Sci, Tampa, FL 33620 USA.
NR 32
TC 1
Z9 1
U1 0
U2 3
PU HUMAN KINETICS PUBL INC
PI CHAMPAIGN
PA 1607 N MARKET ST, PO BOX 5076, CHAMPAIGN, IL 61820-2200 USA
SN 1065-8483
J9 J APPL BIOMECH
JI J. Appl. Biomech.
PD APR
PY 2013
VL 29
IS 2
BP 147
EP 154
PG 8
WC Engineering, Biomedical; Sport Sciences
SC Engineering; Sport Sciences
GA 138WP
UT WOS:000318542000004
PM 22814283
ER
PT J
AU Fraisse, AA
Ade, PAR
Amiri, M
Benton, SJ
Bock, JJ
Bond, JR
Bonetti, JA
Bryan, S
Burger, B
Chiang, HC
Clark, CN
Contaldi, CR
Crill, BP
Davis, G
Dore, O
Farhang, M
Filippini, JP
Fissel, LM
Gandilo, NN
Golwala, S
Gudmundsson, JE
Hasselfield, M
Hilton, G
Holmes, W
Hristov, VV
Irwin, K
Jones, WC
Kuo, CL
MacTavish, CJ
Mason, PV
Montroy, TE
Morford, TA
Netterfield, CB
O'Dea, DT
Rahlin, AS
Reintsema, C
Ruhl, JE
Runyan, MC
Schenker, MA
Shariff, JA
Soler, JD
Trangsrud, A
Tucker, C
Tucker, RS
Turner, AD
Wiebe, D
AF Fraisse, A. A.
Ade, P. A. R.
Amiri, M.
Benton, S. J.
Bock, J. J.
Bond, J. R.
Bonetti, J. A.
Bryan, S.
Burger, B.
Chiang, H. C.
Clark, C. N.
Contaldi, C. R.
Crill, B. P.
Davis, G.
Dore, O.
Farhang, M.
Filippini, J. P.
Fissel, L. M.
Gandilo, N. N.
Golwala, S.
Gudmundsson, J. E.
Hasselfield, M.
Hilton, G.
Holmes, W.
Hristov, V. V.
Irwin, K.
Jones, W. C.
Kuo, C. L.
MacTavish, C. J.
Mason, P. V.
Montroy, T. E.
Morford, T. A.
Netterfield, C. B.
O'Dea, D. T.
Rahlin, A. S.
Reintsema, C.
Ruhl, J. E.
Runyan, M. C.
Schenker, M. A.
Shariff, J. A.
Soler, J. D.
Trangsrud, A.
Tucker, C.
Tucker, R. S.
Turner, A. D.
Wiebe, D.
CA SPIDER Collaboration
TI SPIDER: probing the early Universe with a suborbital polarimeter
SO JOURNAL OF COSMOLOGY AND ASTROPARTICLE PHYSICS
LA English
DT Article
DE CMBR experiments; CMBR polarisation; inflation; physics of the early
universe
ID MICROWAVE BACKGROUND-RADIATION; GALACTIC DUST EMISSION; POWER SPECTRUM;
WMAP OBSERVATIONS; 2003 FLIGHT; POLARIZATION; ANISOTROPY; TELESCOPE;
TEMPERATURE; BOOMERANG
AB We evaluate the ability of SPIDER, a balloon-borne polarimeter, to detect a divergence-free polarization pattern (B-modes) in the cosmic microwave background (CMB). In the inflationary scenario, the amplitude of this signal is proportional to that of the primordial scalar perturbations through the tensor-to-scalar ratio r. We show that the expected level of systematic error in the SPIDER instrument is significantly below the amplitude of an interesting cosmological signal with r = 0.03. We present a scanning strategy that enables us to minimize uncertainty in the reconstruction of the Stokes parameters used to characterize the CMB, while accessing a relatively wide range of angular scales. Evaluating the amplitude of the polarized Galactic emission in the SPIDER field, we conclude that the polarized emission from interstellar dust is as bright or brighter than the cosmological signal at all SPIDER frequencies (90 GHz, 150 GHz, and 280 GHz), a situation similar to that found in the "Southern Hole." We show that two similar to 20-day flights of the SPIDER instrument can constrain the amplitude of the B-mode signal to r < 0.03 (99% CL) even when foreground contamination is taken into account. In the absence of foregrounds, the same limit can be reached after one 20-day flight.
C1 [Fraisse, A. A.; Chiang, H. C.; Gudmundsson, J. E.; Jones, W. C.; Rahlin, A. S.] Princeton Univ, Dept Phys, Princeton, NJ 08544 USA.
[Tucker, C.; SPIDER Collaboration] Cardiff Univ, Sch Phys & Astron, Cardiff CF10 3AX, S Glam, Wales.
[Amiri, M.; Burger, B.; Davis, G.; Hasselfield, M.; Wiebe, D.] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V5Z 1M9, Canada.
[Benton, S. J.; Netterfield, C. B.] Univ Toronto, Dept Phys, Toronto, ON, Canada.
[Bock, J. J.; Crill, B. P.; Dore, O.; Filippini, J. P.; Golwala, S.; Hristov, V. V.; Mason, P. V.; Morford, T. A.; Runyan, M. C.; Schenker, M. A.; Trangsrud, A.; Tucker, R. S.] CALTECH, Dept Phys, Pasadena, CA 91125 USA.
[Bock, J. J.; Bonetti, J. A.; Crill, B. P.; Dore, O.; Holmes, W.; Turner, A. D.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Bond, J. R.; Farhang, M.] Univ Toronto, Canadian Inst Theoret Astrophys, Toronto, ON M5S 1A1, Canada.
[Bryan, S.; Montroy, T. E.; Ruhl, J. E.] Case Western Reserve Univ, Dept Phys, Cleveland, OH 44106 USA.
[Clark, C. N.; Contaldi, C. R.; O'Dea, D. T.] Univ London Imperial Coll Sci Technol & Med, Blackett Lab, London, England.
[Farhang, M.; Fissel, L. M.; Gandilo, N. N.; Netterfield, C. B.; Shariff, J. A.; Soler, J. D.] Univ Toronto, Dept Astron & Astrophys, Toronto, ON, Canada.
[Hilton, G.; Irwin, K.; Reintsema, C.] NIST, Boulder, CO USA.
[Kuo, C. L.] Stanford Univ, Dept Phys, Stanford, CA 94305 USA.
[MacTavish, C. J.] Univ Cambridge, Kavli Inst Cosmol, Cambridge, England.
RP Fraisse, AA (reprint author), Princeton Univ, Dept Phys, Princeton, NJ 08544 USA.
EM afraisse@princeton.edu
FU National Science Foundation [ANT-1043515]; NASA [APRA-NNX07AL64G,
NESSF-NNX10AM55H]; Gordon and Betty Moore Foundation; NSERC; Canadian
Space Agency; CIFAR; Leifur Eiriksson Foundation; NASA Office of Space
Science
FX The SPIDER collaboration gratefully acknowledges the support of the
National Science Foundation (ANT-1043515), NASA (APRA-NNX07AL64G), and
the Gordon and Betty Moore Foundation. Support in Canada is provided by
NSERC, the Canadian Space Agency, and CIFAR. JEG is supported by a grant
from the Leifur Eiriksson Foundation. ASR is supported by NASA
(NESSF-NNX10AM55H). WCJ acknowledges the generous support of the Alfred
P. Sloan Foundation and of the David and Lucile Packard Foundation. Some
of the results in this paper have been derived using the
HEALPix1 [57] package, as well as the FFTW subroutine library
[58]. This research has made use of NASA's Astrophysics Data System. We
acknowledge the use of the Legacy Archive for Microwave Background Data
Analysis (LAMBDA). Support for LAMBDA is provided by the NASA Office of
Space Science.
NR 59
TC 26
Z9 26
U1 0
U2 4
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 1475-7516
J9 J COSMOL ASTROPART P
JI J. Cosmol. Astropart. Phys.
PD APR
PY 2013
IS 4
AR 047
DI 10.1088/1475-7516/2013/04/047
PG 25
WC Astronomy & Astrophysics; Physics, Particles & Fields
SC Astronomy & Astrophysics; Physics
GA 139BJ
UT WOS:000318556200047
ER
PT J
AU Rastatter, L
Kuznetsova, MM
Glocer, A
Welling, D
Meng, X
Raeder, J
Wiltberger, M
Jordanova, VK
Yu, Y
Zaharia, S
Weigel, RS
Sazykin, S
Boynton, R
Wei, H
Eccles, V
Horton, W
Mays, ML
Gannon, J
AF Rastaetter, L.
Kuznetsova, M. M.
Glocer, A.
Welling, D.
Meng, X.
Raeder, J.
Wiltberger, M.
Jordanova, V. K.
Yu, Y.
Zaharia, S.
Weigel, R. S.
Sazykin, S.
Boynton, R.
Wei, H.
Eccles, V.
Horton, W.
Mays, M. L.
Gannon, J.
TI Geospace environment modeling 2008-2009 challenge: D-st index
SO SPACE WEATHER-THE INTERNATIONAL JOURNAL OF RESEARCH AND APPLICATIONS
LA English
DT Article
DE model validation; GEM 2008 challenge
ID IONOSPHERE-THERMOSPHERE MODEL; OUTPUT PARAMETRIC MODELS; MAGNETIC-FIELD
MODEL; NON-LINEAR SYSTEMS; SOLAR-WIND; ELECTRIC-FIELDS; RING CURRENT;
SIMULATION; MAGNETOSPHERE; SUBSTORM
AB This paper reports the metrics-based results of the Dst index part of the 20082009 GEM Metrics Challenge. The 20082009 GEM Metrics Challenge asked modelers to submit results for four geomagnetic storm events and five different types of observations that can be modeled by statistical, climatological or physics-based models of the magnetosphere-ionosphere system. We present the results of 30 model settings that were run at the Community Coordinated Modeling Center and at the institutions of various modelers for these events. To measure the performance of each of the models against the observations, we use comparisons of 1hour averaged model data with the Dst index issued by the World Data Center for Geomagnetism, Kyoto, Japan, and direct comparison of 1minute model data with the 1minute Dst index calculated by the United States Geological Survey. The latter index can be used to calculate spectral variability of model outputs in comparison to the index. We find that model rankings vary widely by skill score used. None of the models consistently perform best for all events. We find that empirical models perform well in general. Magnetohydrodynamics-based models of the global magnetosphere with inner magnetosphere physics (ring current model) included and stand-alone ring current models with properly defined boundary conditions perform well and are able to match or surpass results from empirical models. Unlike in similar studies, the statistical models used in this study found their challenge in the weakest events rather than the strongest events.
C1 [Rastaetter, L.; Kuznetsova, M. M.] NASA, Goddard Space Flight Ctr, Community Coordinated Modeling Ctr, Greenbelt, MD 20770 USA.
[Glocer, A.; Mays, M. L.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20770 USA.
[Welling, D.; Meng, X.] Univ Michigan, Coll Engn, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA.
[Raeder, J.] Univ New Hampshire, Inst Study Earth Oceans & Space, Dept Phys, Durham, NH 03824 USA.
[Wiltberger, M.] Natl Ctr Atmospher Res, Boulder, CO 80307 USA.
[Jordanova, V. K.; Yu, Y.; Zaharia, S.] Los Alamos Natl Lab, Los Alamos, NM USA.
[Weigel, R. S.] George Mason Univ, Dept Computat & Data Sci, Fairfax, VA 22030 USA.
[Sazykin, S.] Rice Univ, Sch Phys Astron & Computat Sci, Houston, TX USA.
[Boynton, R.; Wei, H.] Univ Sheffield, ACSE, Sheffield, S Yorkshire, England.
[Eccles, V.] Space Environm Corp, Providence, UT USA.
[Horton, W.] Univ Texas Austin, Inst Fus Studies, Austin, TX 78712 USA.
[Gannon, J.] US Geol Survey, Golden, CO USA.
RP Rastatter, L (reprint author), NASA, Goddard Space Flight Ctr, Space Weather Lab, Code 674, Greenbelt, MD 20770 USA.
EM lutz.rastaetter@nasa.gov
RI Glocer, Alex/C-9512-2012; Yu, Yiqun/E-2710-2012; Welling,
Daniel/C-1970-2013; Wiltberger, Michael/B-8781-2008; Rastaetter,
Lutz/D-4715-2012; Sazykin, Stanislav/C-3775-2008; Meng,
Xing/A-1929-2016;
OI Glocer, Alex/0000-0001-9843-9094; Yu, Yiqun/0000-0002-1013-6505;
Jordanova, Vania/0000-0003-0475-8743; Wiltberger,
Michael/0000-0002-4844-3148; Rastaetter, Lutz/0000-0002-7343-4147;
Sazykin, Stanislav/0000-0002-9401-4248; Wei,
Hua-Liang/0000-0002-4704-7346
FU Center for Integrated Space Weather Modeling; Science and Technology
Centers program of the National Science Foundation [ATM-0120950];
National Science Foundation
FX Hourly Dst data were obtained from the World Data Center of
Geomagnetism, Kyoto, Japan and 1 minute data were obtained from the
United States Geological Survey (USGS). Both index values include
magnetic data from the following stations: KAK: Kakioka Magnetic
Observatory, Japan Meteorological Agency, Japan, HON, SJG: Honolulu and
San Juan magnetic observatories, USGS, HER: Hermanus Magnetic
Observatory, South African National Space Agency (SANSA). Solar wind
input data for the models (magnetic field and plasma parameters) were
obtained from OMNI (http://omniweb.gsfc.nasa.gov) and CDAweb
(cdaweb.gsfc.nasa.gov) databases. This work was supported by the Center
for Integrated Space Weather Modeling, which is funded by the Science
and Technology Centers program of the National Science Foundation under
agreement number ATM-0120950. The National Center for Atmospheric
Research is sponsored by the National Science Foundation.
NR 69
TC 15
Z9 15
U1 0
U2 11
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 1539-4956
J9 SPACE WEATHER
JI Space Weather
PD APR
PY 2013
VL 11
IS 4
BP 187
EP 205
DI 10.1002/swe.20036
PG 19
WC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology &
Atmospheric Sciences
SC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology &
Atmospheric Sciences
GA 140EH
UT WOS:000318636700008
ER
PT J
AU Adams, JH
Ahmad, S
Albert, JN
Allard, D
Ambrosio, M
Anchordoqui, L
Anzalone, A
Arai, Y
Aramo, C
Asano, K
Ave, M
Barrillon, P
Batsch, T
Bayer, J
Belenguer, T
Bellotti, R
Berlind, AA
Bertaina, M
Biermann, PL
Biktemerova, S
Blaksley, C
Biccki, J
Blin-Bondil, S
Blumer, J
Bobik, P
Bogomilov, M
Bonamente, M
Briggs, MS
Briz, S
Bruno, A
Cafagna, F
Campana, D
Capdevielle, JN
Caruso, R
Casolino, M
Cassardo, C
Castellini, G
Catalano, O
Cellino, A
Chikawa, M
Christi, MJ
Connaughton, V
Cortes, JF
Crawford, HJ
Cremonini, R
Csorna, S
D'Olivo, JC
Dagoret-Campagne, S
de Castro, AJ
De Donato, C
de la Taille, C
del Peral, L
Dell'Oro, A
De Pascale, MP
Di Martino, M
Distratis, G
Dupieux, M
Ebersoldt, A
Ebisuzaki, T
Engel, R
Falk, S
Fang, K
Fenu, F
Fernandez-Gomez, I
Ferrarese, S
Franceschi, A
Fujimoto, J
Galeotti, P
Garipov, G
Geary, J
Giaccari, UG
Giraudo, G
Gonchar, M
Alvarado, CG
Gorodetzky, P
Guarino, F
Guzman, A
Hachisu, Y
Harlov, B
Haungs, A
Carretero, JH
Higashide, K
Iguchi, T
Ikeda, H
Inoue, N
Inoue, S
Insolia, A
Isgro, F
Itow, Y
Joven, E
Judd, EG
Jung, A
Kajino, F
Kajino, T
Kaneko, I
Karadzhov, Y
Karczmarczyk, J
Katahira, K
Kawai, K
Kawasaki, Y
Keilhauer, B
Khrenov, BA
Kim, JS
Kim, SW
Kim, SW
Kleifges, M
Klimov, PA
Ko, SH
Kolev, D
Kreykenbohm, I
Kudela, K
Kurihara, Y
Kuznetsov, E
La Rosa, G
Lee, J
Licandro, J
Lim, H
Lopez, F
Maccarone, MC
Mannheim, K
Marcelli, L
Marini, A
Martin-Chassard, G
Martinez, O
Masciantonio, G
Mase, K
Matev, R
Maurissen, A
Medina-Tanco, G
Mernik, T
Miyamoto, H
Miyazaki, Y
Mizumoto, Y
Modestino, G
Monnier-Ragaigne, D
de los Rios, JAM
Mot, B
Murakami, T
Nagano, M
Nagata, M
Nagataki, S
Nakamura, T
Nam, JW
Nam, S
Nam, K
Napolitano, T
Naumov, D
Neronov, A
Nomoto, K
Ogawa, T
Ohmori, H
Olinto, AV
Orleanski, P
Osteria, G
Pacheco, N
Panasyuk, MI
Parizot, E
Park, IH
Pastircak, B
Patzak, T
Paul, T
Pennypacker, C
Peter, T
Picozza, P
Pollini, A
Prieto, H
Reardon, P
Reinabi, M
Reyes, M
Ricci, M
Rodriguez, I
Frias, MDR
Ronga, F
Rothkaehl, H
Roudil, G
Rusinov, I
Rybczynski, M
Sabau, MD
Cano, GS
Saito, A
Sakaki, N
Sakata, M
Salazar, H
Sanchez, S
Santangelo, A
Cruz, LS
Palomino, MS
Saprykin, O
Sarazin, F
Sato, H
Sato, M
Schanz, T
Schieler, H
Scotti, V
Scuderi, M
Segreto, A
Selmane, S
Semikoz, D
Serra, M
Sharakin, S
Shibata, T
Shimizu, HM
Shinozaki, K
Shirahama, T
Siemieniec-Ozigbio, G
Lopez, HHS
Sledd, J
Slomiriska, K
Sobey, A
Sugiyama, T
Supanitsky, D
Suzuki, M
Szabelska, B
Szabelski, J
Tajima, F
Tajima, N
Tajima, T
Takahashi, Y
Takami, H
Takeda, M
Takizawa, Y
Tenzer, C
Tibolla, O
Tkachev, L
Tomida, T
Tone, N
Trillaud, F
Tsenov, R
Tsuno, K
Tymieniecka, T
Uchihori, Y
Vaduvescu, O
Valdes-Galicia, JF
Vallania, P
Valore, L
Vankova, G
Vigorito, C
Villasenor, L
von Ballmoos, P
Wada, S
Watanabe, J
Watanabe, S
Watts, J
Weber, M
Weiler, TJ
Wibig, T
Wiencke, L
Wille, M
Wilms, J
Wlodarczyk, Z
Yamamoto, T
Yamamoto, Y
Yang, J
Yano, H
Yashin, IV
Yonetoku, D
Yoshida, K
Yoshida, S
Young, R
Zamora, A
Marchi, AZ
AF Adams, J. H., Jr.
Ahmad, S.
Albert, J. -N.
Allard, D.
Ambrosio, M.
Anchordoqui, L.
Anzalone, A.
Arai, Y.
Aramo, C.
Asano, K.
Ave, M.
Barrillon, P.
Batsch, T.
Bayer, J.
Belenguer, T.
Bellotti, R.
Berlind, A. A.
Bertaina, M.
Biermann, P. L.
Biktemerova, S.
Blaksley, C.
Biccki, J.
Blin-Bondil, S.
Bluemer, J.
Bobik, P.
Bogomilov, M.
Bonamente, M.
Briggs, M. S.
Briz, S.
Bruno, A.
Cafagna, F.
Campana, D.
Capdevielle, J. -N.
Caruso, R.
Casolino, M.
Cassardo, C.
Castellini, G.
Catalano, O.
Cellino, A.
Chikawa, M.
Christi, M. J.
Connaughton, V.
Cortes, J. F.
Crawford, H. J.
Cremonini, R.
Csorna, S.
D'Olivo, J. C.
Dagoret-Campagne, S.
de Castro, A. J.
De Donato, C.
de la Taille, C.
del Peral, L.
Dell'Oro, A.
De Pascale, M. P.
Di Martino, M.
Distratis, G.
Dupieux, M.
Ebersoldt, A.
Ebisuzaki, T.
Engel, R.
Falk, S.
Fang, K.
Fenu, F.
Fernandez-Gomez, I.
Ferrarese, S.
Franceschi, A.
Fujimoto, J.
Galeotti, P.
Garipov, G.
Geary, J.
Giaccari, U. G.
Giraudo, G.
Gonchar, M.
Gonzalez Alvarado, C.
Gorodetzky, P.
Guarino, F.
Guzman, A.
Hachisu, Y.
Harlov, B.
Haungs, A.
Hernandez Carretero, J.
Higashide, K.
Iguchi, T.
Ikeda, H.
Inoue, N.
Inoue, S.
Insolia, A.
Isgro, F.
Itow, Y.
Joven, E.
Judd, E. G.
Jung, A.
Kajino, F.
Kajino, T.
Kaneko, I.
Karadzhov, Y.
Karczmarczyk, J.
Katahira, K.
Kawai, K.
Kawasaki, Y.
Keilhauer, B.
Khrenov, B. A.
Kim, Jeong-Sook
Kim, Soon-Wook
Kim, Sug-Whan
Kleifges, M.
Klimov, P. A.
Ko, S. H.
Kolev, D.
Kreykenbohm, I.
Kudela, K.
Kurihara, Y.
Kuznetsov, E.
La Rosa, G.
Lee, J.
Licandro, J.
Lim, H.
Lopez, F.
Maccarone, M. C.
Mannheim, K.
Marcelli, L.
Marini, A.
Martin-Chassard, G.
Martinez, O.
Masciantonio, G.
Mase, K.
Matev, R.
Maurissen, A.
Medina-Tanco, G.
Mernik, T.
Miyamoto, H.
Miyazaki, Y.
Mizumoto, Y.
Modestino, G.
Monnier-Ragaigne, D.
Morales de los Rios, J. A.
Mot, B.
Murakami, T.
Nagano, M.
Nagata, M.
Nagataki, S.
Nakamura, T.
Nam, J. W.
Nam, S.
Nam, K.
Napolitano, T.
Naumov, D.
Neronov, A.
Nomoto, K.
Ogawa, T.
Ohmori, H.
Olinto, A. V.
Orleanski, P.
Osteria, G.
Pacheco, N.
Panasyuk, M. I.
Parizot, E.
Park, I. H.
Pastircak, B.
Patzak, T.
Paul, T.
Pennypacker, C.
Peter, T.
Picozza, P.
Pollini, A.
Prieto, H.
Reardon, P.
Reinabi, M.
Reyes, M.
Ricci, M.
Rodriguez, I.
Rodriguez Frias, M. D.
Ronga, F.
Rothkaehl, H.
Roudil, G.
Rusinov, I.
Rybczynski, M.
Sabau, M. D.
Saez Cano, G.
Saito, A.
Sakaki, N.
Sakata, M.
Salazar, H.
Sanchez, S.
Santangelo, A.
Santiago Cruz, L.
Sanz Palomino, M.
Saprykin, O.
Sarazin, F.
Sato, H.
Sato, M.
Schanz, T.
Schieler, H.
Scotti, V.
Scuderi, M.
Segreto, A.
Selmane, S.
Semikoz, D.
Serra, M.
Sharakin, S.
Shibata, T.
Shimizu, H. M.
Shinozaki, K.
Shirahama, T.
Siemieniec-Ozigbio, G.
Silva Lopez, H. H.
Sledd, J.
Slomiriska, K.
Sobey, A.
Sugiyama, T.
Supanitsky, D.
Suzuki, M.
Szabelska, B.
Szabelski, J.
Tajima, F.
Tajima, N.
Tajima, T.
Takahashi, Y.
Takami, H.
Takeda, M.
Takizawa, Y.
Tenzer, C.
Tibolla, O.
Tkachev, L.
Tomida, T.
Tone, N.
Trillaud, F.
Tsenov, R.
Tsuno, K.
Tymieniecka, T.
Uchihori, Y.
Vaduvescu, O.
Valdes-Galicia, J. F.
Vallania, P.
Valore, L.
Vankova, G.
Vigorito, C.
Villasenor, L.
von Ballmoos, P.
Wada, S.
Watanabe, J.
Watanabe, S.
Watts, J., Jr.
Weber, M.
Weiler, T. J.
Wibig, T.
Wiencke, L.
Wille, M.
Wilms, J.
Wlodarczyk, Z.
Yamamoto, T.
Yamamoto, Y.
Yang, J.
Yano, H.
Yashin, I. V.
Yonetoku, D.
Yoshida, K.
Yoshida, S.
Young, R.
Zamora, A.
Marchi, A. Zuccaro
TI An evaluation of the exposure in nadir observation of the JEM-EUSO
mission
SO ASTROPARTICLE PHYSICS
LA English
DT Article
DE Ultra High Energy Cosmic Rays; Space-based experiment; Extensive air
showers; JEM-EUSO mission
ID EXTENSIVE AIR SHOWERS; ENERGY COSMIC-RAYS; SPACE; RADIATION; SPECTRUM;
DETECTOR; CLOUDS; NM
AB We evaluate the exposure during nadir observations with JEM-EUSO, the Extreme Universe Space Observatory, on-board the Japanese Experiment Module of the International Space Station. Designed as a mission to explore the extreme energy Universe from space, JEM-EUSO will monitor the Earth's nighttime atmosphere to record the ultraviolet light from tracks generated by extensive air showers initiated by ultra-high energy cosmic rays. In the present work, we discuss the particularities of space-based observation and we compute the annual exposure in nadir observation. The results are based on studies of the expected trigger aperture and observational duty cycle, as well as, on the investigations of the effects of clouds and different types of background light. We show that the annual exposure is about one order of magnitude higher than those of the presently operating ground-based observatories. (C) 2013 Elsevier B.V. All rights reserved.
C1 [Bogomilov, M.; Karadzhov, Y.; Kolev, D.; Matev, R.; Rusinov, I.; Tsenov, R.; Vankova, G.] Sofia Univ St Kliment Ohridski, Sofia, Bulgaria.
[Ahmad, S.; Albert, J. -N.; Barrillon, P.; Blin-Bondil, S.; de la Taille, C.; Martin-Chassard, G.; Monnier-Ragaigne, D.; Weiler, T. J.] Univ Paris 11, Lab Accelerateur Lineaire, CNES, IN2P3, Orsay, France.
[Allard, D.; Blaksley, C.; Capdevielle, J. -N.; Gorodetzky, P.; Parizot, E.; Patzak, T.; Selmane, S.; Semikoz, D.] Univ Paris Diderot, APC, CNRS, CEA,Irfu,IN2P3, Sorbonne Paris Cite, France.
[Dupieux, M.; Mot, B.; Roudil, G.; von Ballmoos, P.] Univ Toulouse, CNRS, IRAP, Toulouse, France.
[Kreykenbohm, I.; Wille, M.; Wilms, J.] Univ Erlangen Nurnberg, ECAP, Erlangen, Germany.
[Biermann, P. L.; Bluemer, J.; Ebersoldt, A.; Engel, R.; Falk, S.; Haungs, A.; Keilhauer, B.; Kleifges, M.; Sakaki, N.; Schieler, H.; Scuderi, M.; Weber, M.] Karlsruhe Inst Technol KIT, Karlsruhe, Germany.
[Tajima, T.] Univ Munich, Munich, Germany.
[Bayer, J.; Distratis, G.; Fenu, F.; Guzman, A.; Mernik, T.; Santangelo, A.; Schanz, T.; Tenzer, C.] Univ Tubingen, Kepler Ctr, Inst Astron & Astrophys, Tubingen, Germany.
[Mannheim, K.; Tibolla, O.] Univ Wurzburg, Inst Theoret Phys & Astrophys, Wurzburg, Germany.
[Bruno, A.; Cafagna, F.] Ist Nazl Fis Nucl, Sez Bari, Bari, Italy.
[Bellotti, R.] Univ Bari Aldo Moro, Bari, Italy.
[Bellotti, R.] INFN Sez Bari, Bari, Italy.
[Insolia, A.] Univ Catania, Dipartimento Fis & Astron, I-95124 Catania, Italy.
[Castellini, G.] CNR, Ist Nazl Ott Firenze, Florence, Italy.
[Franceschi, A.; Marini, A.; Modestino, G.; Napolitano, T.; Ricci, M.; Ronga, F.] Ist Nazl Fis Nucl, Lab Nazl Frascati, Frascati, Italy.
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[Guarino, F.; Isgro, F.; Scotti, V.] Univ Naples Federico II, Dipartimento Sci Fis, Naples, Italy.
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[Casolino, M.; De Donato, C.; De Pascale, M. P.; Marcelli, L.; Masciantonio, G.; Picozza, P.] Univ Roma Tor Vergata, Dipartimento Fis, Rome, Italy.
[Bertaina, M.; Cassardo, C.; Cellino, A.; Dell'Oro, A.; Di Martino, M.; Ferrarese, S.; Galeotti, P.; Giraudo, G.; Vallania, P.; Vigorito, C.] Ist Nazl Fis Nucl, Sez Torino, Turin, Italy.
[Bertaina, M.; Cassardo, C.; Cremonini, R.; Ferrarese, S.; Galeotti, P.; Vigorito, C.] Univ Turin, Dipartimento Fis, I-10125 Turin, Italy.
[Cellino, A.; Dell'Oro, A.; Di Martino, M.; Vallania, P.] Osserv Astron Torino, Ist Nazl Astrofis, Turin, Italy.
[Mase, K.; Yoshida, S.] Chiba Univ, Chiba, Japan.
[Uchihori, Y.] Natl Inst Radiol Sci, Chiba 260, Japan.
[Miyazaki, Y.; Nagano, M.] Fukui Univ Technol, Fukui, Japan.
[Chikawa, M.] Kinki Univ, Higashiosaka, Osaka 577, Japan.
[Tajima, F.] Hiroshima Univ, Hiroshima, Japan.
[Murakami, T.; Yonetoku, D.] Kanazawa Univ, Kanazawa, Ishikawa, Japan.
[Takeda, M.] Univ Tokyo, Inst Cosm Ray Res, Kashiwa, Chiba, Japan.
[Nagata, M.] Kobe Univ, Kobe, Hyogo 657, Japan.
[Iguchi, T.; Kajino, F.; Sakata, M.; Sato, H.; Yamamoto, T.; Yamamoto, Y.; Yoshida, K.] Konan Univ, Kobe, Hyogo, Japan.
[Nakamura, T.; Saito, A.] Kyoto Univ, Kyoto, Japan.
[Nagataki, S.] Kyoto Univ, Yukawa Inst, Kyoto, Japan.
[Kajino, T.; Mizumoto, Y.; Watanabe, J.] Natl Astron Observ, Mitaka, Tokyo 181, Japan.
[Shimizu, H. M.; Sugiyama, T.] Nagoya Univ, Nagoya, Aichi 4648601, Japan.
[Itow, Y.] Nagoya Univ, Solar Terr Environm Lab, Nagoya, Aichi 4648601, Japan.
[Ikeda, H.; Suzuki, M.; Yano, H.] Inst Space & Astronaut Sci JAXA, Sagamihara, Kanagawa, Japan.
[Shibata, T.] Aoyama Gakuin Univ, Sagamihara, Kanagawa, Japan.
[Higashide, K.; Inoue, N.; Shirahama, T.] Saitama Univ, Saitama 3388570, Japan.
[Sato, M.; Takahashi, Y.; Watanabe, S.] Hokkaido Univ, Sapporo, Hokkaido, Japan.
[Asano, K.] Tokyo Inst Technol, Interact Res Ctr Sci, Tokyo 152, Japan.
[Inoue, S.; Nomoto, K.] Univ Tokyo, Tokyo, Japan.
[Arai, Y.; Fujimoto, J.; Kurihara, Y.; Takami, H.] High Energy Accelerator Res Org KEK, Tsukuba, Ibaraki, Japan.
[Casolino, M.; Ebisuzaki, T.; Hachisu, Y.; Higashide, K.; Kaneko, I.; Katahira, K.; Kawai, K.; Kawasaki, Y.; Miyamoto, H.; Ogawa, T.; Ohmori, H.; Picozza, P.; Shinozaki, K.; Tajima, N.; Takizawa, Y.; Tomida, T.; Tone, N.; Tsuno, K.; Wada, S.; Marchi, A. Zuccaro] RIKEN Adv Sci Inst, Wako, Saitama, Japan.
[Ko, S. H.] Korea Adv Inst Sci & Technol, Taejon 305701, South Korea.
[Kim, Jeong-Sook; Kim, Soon-Wook] Korea Astron & Space Sci Inst KASI, Taejon, South Korea.
[Jung, A.; Lee, J.; Lim, H.; Nam, J. W.; Nam, S.; Nam, K.; Park, I. H.; Yang, J.] Ewha Womans Univ, Seoul, South Korea.
[Kim, Sug-Whan] Yonsei Univ, Ctr Galaxy Evolut Res, Seoul 120749, South Korea.
[D'Olivo, J. C.; Medina-Tanco, G.; Santiago Cruz, L.; Silva Lopez, H. H.; Supanitsky, D.; Trillaud, F.; Valdes-Galicia, J. F.; Zamora, A.] Univ Nacl Autonoma Mexico, Mexico City, DF, Mexico.
[Villasenor, L.] UMSNH, Morelia, Michoacan, Mexico.
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[Rybczynski, M.; Wlodarczyk, Z.] Jan Kochanowski Univ Humanities & Sci, Inst Phys, Kielce, Poland.
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[Tymieniecka, T.] Cardinal Stefan Wyszyriski Univ, Warsaw, Poland.
[Biccki, J.; Orleanski, P.; Rothkaehl, H.; Slomiriska, K.] Polish Acad Sci CBK, Space Res Ctr, Warsaw, Poland.
[Biktemerova, S.; Gonchar, M.; Naumov, D.; Tkachev, L.] Joint Inst Nucl Res, Dubna, Russia.
[Harlov, B.; Saprykin, O.] TsNIIMash, Cent Res Inst Machine Bldg, Korolev, Russia.
[Garipov, G.; Khrenov, B. A.; Klimov, P. A.; Panasyuk, M. I.; Sharakin, S.; Yashin, I. V.] Moscow MV Lomonosov State Univ, Skobeltsyn Inst Nucl Phys, Moscow 117234, Russia.
[Bobik, P.; Kudela, K.; Pastircak, B.] Slovak Acad Sci, Inst Expt Phys, Kosice 04353, Slovakia.
[Prieto, H.] CSIC, Madrid, Spain.
[Belenguer, T.; Gonzalez Alvarado, C.; Reinabi, M.; Sabau, M. D.; Sanz Palomino, M.] INTA, Madrid, Spain.
[Pacheco, N.] Univ Autonoma Madrid, Inst Fis Teor, E-28049 Madrid, Spain.
[del Peral, L.; Hernandez Carretero, J.; Morales de los Rios, J. A.; Prieto, H.; Rodriguez Frias, M. D.; Saez Cano, G.] Univ Alcala UAH, Madrid, Spain.
[Briz, S.; Cortes, J. F.; de Castro, A. J.; Fernandez-Gomez, I.; Lopez, F.; Rodriguez, I.; Sanchez, S.] Univ Carlos III Madrid, E-28903 Getafe, Spain.
[Ave, M.] Univ Santiago de Compostela, Santiago De Compostela, Spain.
[Joven, E.; Licandro, J.; Reyes, M.; Serra, M.; Vaduvescu, O.] IAC, Tenerife, Spain.
[Maurissen, A.; Pollini, A.] Swiss Ctr Elect & Microtechnol CSEM, Neuchatel, Switzerland.
[Neronov, A.] ISDC Data Ctr Astrophys, Versoix, Switzerland.
[Peter, T.] ETH, Inst Atmospher & Climate Sci, Zurich, Switzerland.
[Crawford, H. J.; Judd, E. G.; Pennypacker, C.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
[Fang, K.; Olinto, A. V.] Univ Chicago, Chicago, IL 60637 USA.
[Sarazin, F.; Wiencke, L.] Colorado Sch Mines, Golden, CO 80401 USA.
[Adams, J. H., Jr.; Bonamente, M.; Briggs, M. S.; Connaughton, V.; Geary, J.; Kuznetsov, E.; Reardon, P.; Watts, J., Jr.] Univ Alabama, Huntsville, AL 35899 USA.
[Anchordoqui, L.; Paul, T.] Univ Wisconsin, Milwaukee, WI 53201 USA.
[Christi, M. J.; Sledd, J.; Sobey, A.; Young, R.] NASA, George C Marshall Space Flight Ctr, Washington, DC USA.
[Berlind, A. A.; Csorna, S.] Vanderbilt Univ, Nashville, TN USA.
RP Bertaina, M (reprint author), Univ Turin, Dipartimento Fis, I-10125 Turin, Italy.
EM bertaina@to.infn.it; kenjikry@riken.jp
RI scuderi, mario/O-7019-2014; Guarino, Fausto/I-3166-2012; marcelli,
laura/K-8860-2016; Rodriguez Frias, Maria /A-7608-2015; Briz,
Susana/G-7732-2015; Ko, Seung Hwan/B-5448-2008; Insolia,
Antonio/M-3447-2015; Cellino, Alberto/N-1570-2015; Kreykenbohm,
Ingo/H-9659-2013; Ko, Seung Hwan/C-2043-2011; Klimov, Pavel/E-2783-2012;
Wilms, Joern/C-8116-2013; Panasyuk, Mikhail/E-2005-2012; Cafagna,
Francesco/A-9299-2010; Ebisuzaki, Toshikazu/N-6998-2014; Ohmori ,
Hitoshi /A-7562-2015; LOPEZ, FERNANDO/H-5071-2015; De Donato,
Cinzia/J-9132-2015
OI Aramo, Carla/0000-0002-8412-3846; Bertaina, Mario
Edoardo/0000-0003-1069-1397; Dell'Oro, Aldo/0000-0003-1561-9685;
Anzalone, Anna/0000-0003-1849-198X; Bellotti,
Roberto/0000-0003-3198-2708; Vallania, Piero/0000-0001-9089-7875; La
Rosa, Giovanni/0000-0002-3931-2269; Modestino,
Giuseppina/0000-0003-1556-3917; Cassardo, Claudio/0000-0001-5212-3211;
casolino, marco/0000-0001-6067-5104; Catalano,
Osvaldo/0000-0002-9554-4128; Segreto, Alberto/0000-0001-7341-6603;
Maccarone, Maria Concetta/0000-0001-8722-0361; Isgro,
Francesco/0000-0001-9342-5291; Castellini, Guido/0000-0002-0177-0643;
Naumov, Dmitry Vadimovich/0000-0002-0966-8803; Picozza,
Piergiorgio/0000-0002-7986-3321; scuderi, mario/0000-0001-9026-5317;
Guarino, Fausto/0000-0003-1427-9885; marcelli,
laura/0000-0002-3180-1228; Rodriguez Frias, Maria /0000-0002-2550-4462;
Briz, Susana/0000-0001-5963-3257; Wibig, Tadeusz/0000-0002-2078-0580;
Weiler, Thomas/0000-0002-0885-1868; Franceschi, Massimo
Alberto/0000-0002-8222-7000; Masciantonio, Giuseppe/0000-0002-8911-1561;
Del Peral, Luis/0000-0003-2580-5668; Ko, Seung Hwan/0000-0002-7477-0820;
Insolia, Antonio/0000-0002-9040-1566; Cellino,
Alberto/0000-0002-6645-334X; Kreykenbohm, Ingo/0000-0001-7335-1803;
Klimov, Pavel/0000-0001-9815-6123; Wilms, Joern/0000-0003-2065-5410;
Cafagna, Francesco/0000-0002-7450-4784; Ebisuzaki,
Toshikazu/0000-0002-3918-1166; LOPEZ, FERNANDO/0000-0003-4723-0535; De
Donato, Cinzia/0000-0002-9725-1281
FU RIKEN; JSPS KAKENHI [22340063, 23340081, 24244042]; Italian Ministry of
Foreign Affairs, General Direction for the Cultural Promotion and
Cooperation; Helmholtz Alliance for Astroparticle Physics HAP; Helmholtz
Association, Germany; Slovak Academy of Sciences MVTS JEM-EUSO; VEGA
grant agency [2/0081/10]; MICINN [AYA2009-06037-E/ESP, AYA-ESP
2010-19082, AYA2011-29489-C03-01, AYA2012-39115-C03-01, CSD2009-00064];
Comunidad de Madrid (CAM) [S2009/ESP-1496]
FX This work was partially supported by Basic Science Interdisciplinary
Research Projects of RIKEN and JSPS KAKENHI Grant (22340063, 23340081,
and 24244042), by the Italian Ministry of Foreign Affairs, General
Direction for the Cultural Promotion and Cooperation, by the 'Helmholtz
Alliance for Astroparticle Physics HAP' funded by the Initiative and
Networking Fund of the Helmholtz Association, Germany, and by Slovak
Academy of Sciences MVTS JEM-EUSO as well as VEGA grant agency project
2/0081/10. The Spanish Consortium involved in the JEM-EUSO Space Mission
is funded by MICINN under projects AYA2009-06037-E/ESP, AYA-ESP
2010-19082, AYA2011-29489-C03-01, AYA2012-39115-C03-01, CSD2009-00064
(Consolider MULTIDARK) and by Comunidad de Madrid (CAM) under project
S2009/ESP-1496.
NR 53
TC 55
Z9 55
U1 2
U2 53
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0927-6505
EI 1873-2852
J9 ASTROPART PHYS
JI Astropart Phys.
PD APR
PY 2013
VL 44
BP 76
EP 90
DI 10.1016/j.astropartphys.2013.01.008
PG 15
WC Astronomy & Astrophysics; Physics, Particles & Fields
SC Astronomy & Astrophysics; Physics
GA 135WT
UT WOS:000318322100009
ER
PT J
AU Hoffmayer, ER
Franks, JS
Driggers, WB
Howey, PW
AF Hoffmayer, Eric R.
Franks, James S.
Driggers, William B., III
Howey, Paul W.
TI DIEL VERTICAL MOVEMENTS OF A SCALLOPED HAMMERHEAD, SPHYRNA LEWINI, IN
THE NORTHERN GULF OF MEXICO
SO BULLETIN OF MARINE SCIENCE
LA English
DT Article
ID SATELLITE ARCHIVAL TAGS; TUNA THUNNUS-THYNNUS; PACIFIC-OCEAN; SHARKS;
CALIFORNIA; FISH; TEMPERATURE; AUSTRALIA; TRACKING; MOKARRAN
AB Despite the circumglobal distribution of scalloped hammerheads, Sphyrna lewini (Griffith and Smith, 1834), little information is available regarding fine-scale movement and habitat use patterns for this species. Over a 27-d period, data were collected on diel habitat use and environmental preferences of a 240 cm (total length) female S. lewini. The shark exhibited a consistent and repeated diel vertical movement pattern, making more than 76 deep nighttime dives; the maximum depth reached was 964 m, where the temperature was 5.8 degrees C. The purpose of the nightly oscillatory deep diving pattern is unknown but could possibly represent feeding behavior. These findings represent the first detailed account of S. lewini diel vertical behavior and habitat utilization in the western North Atlantic Ocean.
C1 [Hoffmayer, Eric R.; Driggers, William B., III] Natl Marine Fisheries Serv, Southeast Fisheries Sci Ctr, Mississippi Labs, Pascagoula, MS 39567 USA.
[Franks, James S.] Univ So Mississippi, Gulf Coast Res Lab, Ctr Fisheries Res & Dev, Ocean Springs, MS 39564 USA.
[Howey, Paul W.] Microwave Telemetry Inc, Columbia, MD 21045 USA.
RP Hoffmayer, ER (reprint author), Natl Marine Fisheries Serv, Southeast Fisheries Sci Ctr, Mississippi Labs, PO Drawer 1207, Pascagoula, MS 39567 USA.
EM eric.hoffmayer@noaa.gov
RI sebastianovitsch, stepan/G-8507-2013
FU US National Marine Fisheries Service [NA08NMF4540389]
FX We extend our appreciation to B Delabar and BC Bobby of the sport
fishing vessel FRENZY (Venice, Louisiana). We also thank R Berg (BEI,
Inc.) for providing video of the scalloped hammerhead aggregation at
MC582 the day prior to our tagging event. G Parsons provided valuable
comments on an earlier version of the manuscript. This research was
partially supported by US National Marine Fisheries Service, Cooperative
Research Program, Grant #NA08NMF4540389 to E Hoffmayer and J Franks.
This research was conducted in compliance with US law under Scientific
Research Permit HMS-EFP-08-07, issued by the Highly Migratory Species
Division of the Office of Sustainable Fisheries, National Marine
Fisheries Service, Silver Spring, MD 20910, USA, and the Institutional
Animal Care and Use Committee of the University of Southern Mississippi
(protocol 09031204). Mention of commercial products does not imply
endorsement by the University of Southern Mississippi or the National
Marine Fisheries Service.
NR 22
TC 5
Z9 6
U1 3
U2 38
PU ROSENSTIEL SCH MAR ATMOS SCI
PI MIAMI
PA 4600 RICKENBACKER CAUSEWAY, MIAMI, FL 33149 USA
SN 0007-4977
J9 B MAR SCI
JI Bull. Mar. Sci.
PD APR
PY 2013
VL 89
IS 2
BP 551
EP 557
DI 10.5343/bms.2012.1048
PG 7
WC Marine & Freshwater Biology; Oceanography
SC Marine & Freshwater Biology; Oceanography
GA 136QM
UT WOS:000318378500009
ER
PT J
AU Angal, A
Xiong, XX
Wu, AS
Chander, G
Choi, T
AF Angal, Amit
Xiong, Xiaoxiong
Wu, Aisheng
Chander, Gyanesh
Choi, Taeyoung
TI Multitemporal Cross-Calibration of the Terra MODIS and Landsat 7 ETM+
Reflective Solar Bands
SO IEEE TRANSACTIONS ON GEOSCIENCE AND REMOTE SENSING
LA English
DT Article
DE Cross-calibration; landsat ETM; Libya-4; MODTRAN; MODIS; water-vapor
ID NEAR-INFRARED CHANNELS; SATELLITE SENSORS; DESERT SITES; WATER-VAPOR;
PERFORMANCE; AVHRR; MODEL
AB In recent years, there has been a significant increase in the use of remotely sensed data to address global issues. With the open data policy, the data from the Moderate Resolution Imaging Spectroradiometer (MODIS) and Enhanced Thematic Mapper Plus (ETM+) sensors have become a critical component of numerous applications. These two sensors have been operational for more than a decade, providing a rich archive of multispectral imagery for analysis of mutitemporal remote sensing data. This paper focuses on evaluating the radiometric calibration agreement between MODIS and ETM+ using the near-simultaneous and cloud-free image pairs over an African pseudo-invariant calibration site, Libya 4. To account for the combined uncertainties in the top-of-atmosphere (TOA) reflectance due to surface and atmospheric bidirectional reflectance distribution function (BRDF), a semiempirical BRDF model was adopted to normalize the TOA reflectance to the same illumination and viewing geometry. In addition, the spectra from the Earth Observing-1 (EO-1) Hyperion were used to compute spectral corrections between the corresponding MODIS and ETM+ spectral bands. As EO-1 Hyperion scenes were not available for all MODIS and ETM+ data pairs, MODerate resolution atmospheric TRANsmission (MODTRAN) 5.0 simulations were also used to adjust for differences due to the presence or lack of absorption features in some of the bands. A MODIS split-window algorithm provides the atmospheric water vapor column abundance during the overpasses for the MODTRAN simulations. Additionally, the column atmospheric water vapor content during the overpass was retrieved using the MODIS precipitable water vapor product. After performing these adjustments, the radiometric cross-calibration of the two sensors was consistent to within 7%. Some drifts in the response of the bands are evident, with MODIS band 3 being the largest of about 6% over 10 years, a change that will be corrected in Collection 6 MODIS processing.
C1 [Angal, Amit] Sci Syst & Applicat Inc, Lanham, MD 20706 USA.
[Xiong, Xiaoxiong] NASA, Goddard Space Flight Ctr, Sci & Explorat Directorate, Greenbelt, MD 20771 USA.
[Wu, Aisheng; Choi, Taeyoung] Sigma Space Co, Lanham, MD 20706 USA.
[Chander, Gyanesh] SGT Inc, Greenbelt, MD 20770 USA.
RP Angal, A (reprint author), Sci Syst & Applicat Inc, Lanham, MD 20706 USA.
EM amit.angal@ssaihq.com; Xiaoxiong.Xiong-1@nasa.gov; wu@sigmaspace.com;
gchander@usgs.gov; tchoi@sigmaspace.com
RI Trivedi, Kruti/E-7558-2015; Choi, Taeyoung/E-4437-2016; Richards,
Amber/K-8203-2015
OI Choi, Taeyoung/0000-0002-4596-989X;
FU U.S. Geological Survey [G10PC00044]
FX The authors would like to thank T. Adamson (SGT) for providing helpful
comments in the technical review of this paper. The work performed by G.
Chander is under U.S. Geological Survey contract G10PC00044. The
detailed comments from the anonymous reviewers were extremely helpful in
improving the quality and readability of this paper.
NR 25
TC 14
Z9 14
U1 3
U2 30
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 0196-2892
J9 IEEE T GEOSCI REMOTE
JI IEEE Trans. Geosci. Remote Sensing
PD APR
PY 2013
VL 51
IS 4
SI SI
BP 1870
EP 1882
DI 10.1109/TGRS.2012.2235448
PN 1
PG 13
WC Geochemistry & Geophysics; Engineering, Electrical & Electronic; Remote
Sensing; Imaging Science & Photographic Technology
SC Geochemistry & Geophysics; Engineering; Remote Sensing; Imaging Science
& Photographic Technology
GA 137HN
UT WOS:000318426400002
ER
PT J
AU Zhao, JJ
Wang, YQ
Hashimoto, H
Melton, FS
Hiatt, SH
Zhang, HY
Nemani, RR
AF Zhao, Jianjun
Wang, Yeqiao
Hashimoto, Hirofumi
Melton, Forrest S.
Hiatt, Samuel H.
Zhang, Hongyan
Nemani, Ramakrishna R.
TI The Variation of Land Surface Phenology From 1982 to 2006 Along the
Appalachian Trail
SO IEEE TRANSACTIONS ON GEOSCIENCE AND REMOTE SENSING
LA English
DT Article
DE Appalachian Trail (AT); climatic variation; Global Inventory Modeling
and Mapping Studies (GIMMS); land surface phenology (LSP); Surface
Observation and Gridding System (SOGS)
ID NDVI TIME-SERIES; SATELLITE SENSOR DATA; SPRING PHENOLOGY; PLANT
PHENOLOGY; HIGH-LATITUDES; COVER CHANGE; MODIS; DYNAMICS; SEASONALITY;
FORESTS
AB The gradients of the Appalachian Trail (A.T.) in elevations and latitudes provide a megatransect to study environmental variations in the eastern United States. This paper reveals patterns and trends of land surface phenology (LSP) in association with climatic variables within a corridor area along the A. T. We employed time-series data from Global Inventory Modeling and Mapping Studies and the Surface Observation and Gridding System between 1982 and 2006 to extract spatial and temporal variation patterns of LSP metrics and the correlations with meteorological parameters. The derived trends in LSP metrics indicate that the extended length of season mainly resulted from delayed end of season (EOS) across the study area. More significant change occurred in the northern segment than in the southern segment, which reflects latitudinal effects. We analyzed the relationship between LSP and longitude, latitude, elevation, local climatic variables, and large-scale climate oscillations. Delayed start of season in 1989 and advanced EOS in 1988 were observed responding to the La Nina episode during 1988-1989. This paper provides information about the effects of climate and topography on LSP along the Appalachian Mountain ridges.
C1 [Zhao, Jianjun; Zhang, Hongyan] NE Normal Univ, Sch Urban & Environm Sci, Changchun 130024, Peoples R China.
[Zhao, Jianjun; Wang, Yeqiao] Univ Rhode Isl, Dept Nat Resources Sci, Kingston, RI 02881 USA.
[Hashimoto, Hirofumi; Melton, Forrest S.] Calif State Univ, Div Sci & Environm Policy, Monterey, CA 93955 USA.
[Hashimoto, Hirofumi; Melton, Forrest S.; Hiatt, Samuel H.; Nemani, Ramakrishna R.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
RP Zhao, JJ (reprint author), NE Normal Univ, Sch Urban & Environm Sci, Changchun 130024, Peoples R China.
EM zhaojj662@gmail.com; yqwang@mail.uri.edu; hirofumi.hashimoto@gmail.com;
forrest.s.melton@nasa.gov; samhiatt@gmail.com; zhy@nenu.edu.cn;
rama.nemani@nasa.gov
FU NASA Science Mission Directorate (ROSES) [NNX09AV82G]
FX This work was a component of the project titled "A Decision Support
System for Monitoring, Reporting and Forecasting Ecological Conditions
of the Appalachian National Scenic Trail," which was supported by NASA
Science Mission Directorate (ROSES-2008) under Decision Support through
Earth Science Research Results (Grant NNX09AV82G).
NR 53
TC 6
Z9 6
U1 1
U2 25
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 0196-2892
J9 IEEE T GEOSCI REMOTE
JI IEEE Trans. Geosci. Remote Sensing
PD APR
PY 2013
VL 51
IS 4
SI SI
BP 2087
EP 2095
DI 10.1109/TGRS.2012.2217149
PN 1
PG 9
WC Geochemistry & Geophysics; Engineering, Electrical & Electronic; Remote
Sensing; Imaging Science & Photographic Technology
SC Geochemistry & Geophysics; Engineering; Remote Sensing; Imaging Science
& Photographic Technology
GA 137HN
UT WOS:000318426400020
ER
PT J
AU Connor, LN
Farrell, SL
McAdoo, DC
Krabill, WB
Manizade, S
AF Connor, Laurence N.
Farrell, Sinead Louise
McAdoo, David C.
Krabill, William B.
Manizade, Serdar
TI Validating ICESat Over Thick Sea Ice in the Northern Canada Basin
SO IEEE TRANSACTIONS ON GEOSCIENCE AND REMOTE SENSING
LA English
DT Article
DE Altimetry; laser radar; satellite applications; sea ice; snow
ID LASER ALTIMETER MEASUREMENTS; AIRBORNE LASER; RADAR ALTIMETER; SNOW;
FREEBOARD; VARIABILITY; MOTION; OCEAN; COVER; LAND
AB Only in the past eight years has the feasibility of using satellite-borne altimeters to estimate sea ice freeboard and thickness been demonstrated, and these estimates still have uncertainties primarily associated with limited knowledge of snow loading on sea ice. Because accurate estimates of Arctic-wide sea ice thickness and volume are fundamental inputs to global climate models, validation of satellite-derived thickness estimates using independent data is required. A detailed assessment of freeboard retrieved by the Geoscience Laser Altimeter System (GLAS) aboard the Ice, Cloud, and land Elevation Satellite has been carried out using high-resolution laser altimetry from the National Aeronautics and Space Administration's Airborne Topographic Mapper (ATM), the Delay-Doppler radar altimeter, and digital photography collected along a 300-km segment of sea ice in the Canada Basin. Exploiting the repeat coverage of the aircraft flight line, a correction was applied to GLAS footprint geolocations to adjust for sea ice drift that occurred during the time between satellite and aircraft acquisitions. Comparisons of GLAS and ATM measurements over sea ice show excellent agreement (about a 0.00-m mean) with no apparent bias between data sets. Freeboard estimates were examined using data from GLAS and ATM independently, employing measurements over refrozen leads to estimate local sea surface heights (SSHs). The results demonstrate the sensitivity of freeboard and thickness calculations to an accurate estimation of local SSH. Snow depth derived by differencing laser and radar data was combined with the freeboard estimates to yield a mean sea ice thickness of similar to 5.5mover a 250-km subsection of the flight track.
C1 [Connor, Laurence N.; McAdoo, David C.] NOAA, Lab Satellite Altimetry, Natl Environm Satellite Data & Informat Serv, Ctr Satellite Applicat & Res, College Pk, MD 20740 USA.
[Farrell, Sinead Louise] Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20740 USA.
[Farrell, Sinead Louise] NOAA, Lab Satellite Altimetry, NESDIS, STAR, College Pk, MD 20740 USA.
[Krabill, William B.] NASA, Sigma Space Inc, Wallops Flight Facil, Wallops Isl, VA 23337 USA.
[Manizade, Serdar] NASA, URS Corp, Wallops Flight Facil, Wallops Isl, VA 23337 USA.
RP Connor, LN (reprint author), NOAA, Lab Satellite Altimetry, Natl Environm Satellite Data & Informat Serv, Ctr Satellite Applicat & Res, College Pk, MD 20740 USA.
EM Laurence.Connor@noaa.gov; Sineadf@umd.edu; Dave.McAdoo@noaa.gov;
William.B.Krabill@nasa.gov; Serdar.Manizade@nasa.gov
RI Farrell, Sinead/F-5586-2010; McAdoo, Dave/F-5612-2010; Connor,
Laurence/E-7930-2011
OI Farrell, Sinead/0000-0003-3222-2751; McAdoo, Dave/0000-0002-7533-5564;
Connor, Laurence/0000-0002-5276-6257
FU National Oceanic and Atmospheric Administration; National Aeronautics
and Space Administration; National Oceanic and Atmospheric
Administration (NOAA)'s Ocean Remote Sensing program; NASA's Cryosphere
Program
FX This work was supported in part by the National Oceanic and Atmospheric
Administration and in part by the National Aeronautics and Space
Administration. The views, opinions, and findings contained in this
report are those of the authors and should not be construed as an
official NOAA or U. S. Government position, policy, or decision.; The
authors would like to thank the National Aeronautics and Space
Administration (NASA) P3 aircrew for their support during the Arctic
Aircraft Altimeter (AAA) 2006 campaign. The March 27, 2006, AAA flight
was supported by the National Oceanic and Atmospheric Administration
(NOAA)'s Ocean Remote Sensing program and NASA's Cryosphere Program. The
authors would also like to thank C. Leuschen for providing the processed
Delay-Doppler data for the AAA flights, the reviewers for their efforts
and insightful suggestions, and NASA's Ice, Cloud, and land Elevation
Satellite (ICESat) Science Project and National Snow and Ice Data Center
for the distribution of the ICESat data (see
http://nsidc.org/data/icesat/). Moderate Resolution Imaging
Spectroradiometer imagery was obtained from NASA's Level 1 and
Atmosphere Archive and Distribution System
(http://ladsweb.nascom.nasa.gov).
NR 46
TC 7
Z9 7
U1 0
U2 15
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 0196-2892
EI 1558-0644
J9 IEEE T GEOSCI REMOTE
JI IEEE Trans. Geosci. Remote Sensing
PD APR
PY 2013
VL 51
IS 4
BP 2188
EP 2200
DI 10.1109/TGRS.2012.2211603
PN 2
PG 13
WC Geochemistry & Geophysics; Engineering, Electrical & Electronic; Remote
Sensing; Imaging Science & Photographic Technology
SC Geochemistry & Geophysics; Engineering; Remote Sensing; Imaging Science
& Photographic Technology
GA 137HY
UT WOS:000318427500004
ER
PT J
AU Tombesi, F
Cappi, M
Reeves, JN
Nemmen, RS
Braito, V
Gaspari, M
Reynolds, CS
AF Tombesi, F.
Cappi, M.
Reeves, J. N.
Nemmen, R. S.
Braito, V.
Gaspari, M.
Reynolds, C. S.
TI Unification of X-ray winds in Seyfert galaxies: from ultra-fast outflows
to warm absorbers
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE accretion, accretion discs; black hole physics; galaxies: active;
galaxies: Seyfert; X-rays: galaxies.
ID ACTIVE GALACTIC NUCLEI; XMM-NEWTON OBSERVATION; SUPERMASSIVE
BLACK-HOLES; RADIO-QUIET AGNS; TRANSMISSION GRATING SPECTROMETER;
ACCRETION DISC OUTFLOWS; SHELL ABSORPTION-LINES; DEEP CHANDRA ACIS;
EMISSION-LINE; PHYSICAL CONDITIONS
AB The existence of ionized X-ray absorbing layers of gas along the line of sight to the nuclei of Seyfert galaxies is a well established observational fact. This material is systematically outflowing and shows a large range in parameters. However, its actual nature and dynamics are still not clear. In order to gain insights into these important issues we performed a literature search for papers reporting the parameters of the soft X-ray warm absorbers (WAs) in 35 type 1 Seyferts and compared their properties to those of the ultra-fast outflows (UFOs) detected in the same sample. The fraction of sources with WAs is >60 per cent, consistent with previous studies. The fraction of sources with UFOs is >34 per cent, >67 per cent of which also show WAs. The large dynamic range obtained when considering all the absorbers together, spanning several orders of magnitude in ionization, column, velocity and distance allows us, for the first time, to investigate general relations among them. In particular, we find significant correlations indicating that the closer the absorber is to the central black hole, the higher the ionization, column, outflow velocity and consequently the mechanical power. In all the cases, the absorbers continuously populate the whole parameter space, with the WAs and the UFOs lying always at the two ends of the distribution. These evidence strongly suggest that these absorbers, often considered of different types, could actually represent parts of a single large-scale stratified outflow observed at different locations from the black hole. The UFOs are likely launched from the inner accretion disc and the WAs at larger distances, such as the outer disc and/or torus. We argue that the observed parameters and correlations are, to date, consistent with both radiation pressure through Compton scattering and magnetohydrodynamic processes contributing to the outflow acceleration, the latter playing a major role. Most of the absorbers, especially the UFOs, show a sufficiently high mechanical power (at least similar to 0.5 per cent of the bolometric luminosity) to provide a significant contribution to active galactic nuclei (AGN) feedback and thus to the evolution of the host galaxy. In this regard, we find possible evidence for the interaction of the AGN wind with the surrounding environment on large scales.
C1 [Tombesi, F.; Nemmen, R. S.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Tombesi, F.; Reynolds, C. S.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Cappi, M.] INAF IASF Bologna, I-40129 Bologna, Italy.
[Reeves, J. N.] Keele Univ, Sch Phys & Geog Sci, Astrophys Grp, Keele ST5 5BG, Staffs, England.
[Braito, V.] INAF Osservatorio Astron Brera, I-23807 Merate, Italy.
[Gaspari, M.] Max Planck Inst Astrophys, D-85741 Garching, Germany.
RP Tombesi, F (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
EM ftombesi@astro.umd.edu
RI Nemmen, Rodrigo/O-6841-2014; Cappi, Massimo/F-4813-2015;
OI Braito, Valentina/0000-0002-2629-4989; Cappi,
Massimo/0000-0001-6966-8920
FU ASI [ASI/INAF/I/009/10/0]; INAF [PRIN-INAF-2011]
FX The authors thank the anonymous referee for the positive and
constructive comments. FT thanks D. Kazanas, K. Fukumura, R. F.
Mushotzky for the useful discussions. MC acknowledges financial support
from ASI (contract ASI/INAF/I/009/10/0) and INAF (contract
PRIN-INAF-2011). RN was supported by an appointment to the NASA
Postdoctoral Program at Goddard Space Flight Center, administered by Oak
Ridge Associated Universities through a contract with NASA. This
research made use of the StatCodes statistical software hosted by Penn
State's Center for Astrostatistics. This research has made use of data
obtained from the High Energy Astrophysics Science Archive Research
Center (HEASARC), provided by NASA's Goddard Space Flight Center. This
research has made use of the NASA/IPAC Extragalactic Database (NED)
which is operated by the Jet Propulsion Laboratory, California Institute
of Technology, under contract with the National Aeronautics and Space
Administration. This research has made use of NASA's Astrophysics Data
System.
NR 128
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PU OXFORD UNIV PRESS
PI OXFORD
PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND
SN 0035-8711
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD APR
PY 2013
VL 430
IS 2
BP 1102
EP 1117
DI 10.1093/mnras/sts692
PG 16
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 135FY
UT WOS:000318275000029
ER
PT J
AU Rostem, K
Chuss, DT
Lourie, NP
Voellmer, GM
Wollack, EJ
AF Rostem, K.
Chuss, D. T.
Lourie, N. P.
Voellmer, G. M.
Wollack, E. J.
TI A waveguide-coupled thermally isolated radiometric source
SO REVIEW OF SCIENTIFIC INSTRUMENTS
LA English
DT Article
ID HEAT; CONDUCTIVITY; NOISE; EPOXY
AB The design and validation of a dual polarization source for waveguide-coupled millimeter and sub-millimeter wave cryogenic sensors is presented. The thermal source is a waveguide mounted absorbing conical dielectric taper. The absorber is thermally isolated with a kinematic suspension that allows the guide to be heat sunk to the lowest bath temperature of the cryogenic system. This approach enables the thermal emission from the metallic waveguide walls to be subdominant to that from the source. The use of low thermal conductivity Kevlar threads for the kinematic mount effectively decouples the absorber from the sensor cold stage. Hence, the absorber can be heated to significantly higher temperatures than the sensor with negligible conductive loading. The kinematic suspension provides high mechanical repeatability and reliability with thermal cycling. A 33-50 GHz blackbody source demonstrates an emissivity of 0.999 over the full waveguide band where the dominant deviation from unity arises from the waveguide ohmic loss. The observed thermal time constant of the source is 40 s when the absorber temperature is 15 K. The specific heat of the lossy dielectric, MF-117, is well approximated by C-v(T) = 0.12 T-2.06 mJ g(-1) K-1 between 3.5 K and 15 K. [http://dx.doi.org/10.1063/1.4795556]
C1 [Rostem, K.; Chuss, D. T.; Lourie, N. P.; Voellmer, G. M.; Wollack, E. J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Rostem, K (reprint author), NASA, Goddard Space Flight Ctr, 8800 Greenbelt Rd, Greenbelt, MD 20771 USA.
RI Wollack, Edward/D-4467-2012
OI Wollack, Edward/0000-0002-7567-4451
FU NASA ROSES/APRA program
FX We gratefully acknowledge financial support from the NASA ROSES/APRA
program. K. Rostem was supported by an appointment to the NASA
Postdoctoral Program at Goddard Space Flight Center. We thank Paul
Cursey for fabrication and metrology support.
NR 27
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U2 3
PU AMER INST PHYSICS
PI MELVILLE
PA CIRCULATION & FULFILLMENT DIV, 2 HUNTINGTON QUADRANGLE, STE 1 N O 1,
MELVILLE, NY 11747-4501 USA
SN 0034-6748
J9 REV SCI INSTRUM
JI Rev. Sci. Instrum.
PD APR
PY 2013
VL 84
IS 4
AR 044701
DI 10.1063/1.4795556
PG 6
WC Instruments & Instrumentation; Physics, Applied
SC Instruments & Instrumentation; Physics
GA 134UQ
UT WOS:000318240900041
PM 23635214
ER
PT J
AU Wang, DH
Liu, Y
Zhu, P
Yin, JF
Li, XF
Tao, WK
AF Wang Donghai
Liu Ying
Zhu Ping
Yin Jinfang
Li Xiaofan
Tao Wei-Kuo
TI Cloud microphysical budget associated with torrential rainfall during
the landfall of severe tropical storm Bilis (2006)
SO ACTA METEOROLOGICA SINICA
LA English
DT Article
DE cloud radiation effects; cloud-radiation interaction; ice clouds; cloud
microphysical budget; torrential rainfall
ID MICROSCALE STRUCTURE; STRATIFORM REGIONS; FRONTAL RAINBANDS;
PRECIPITATION; RADIATION; MESOSCALE; RESPONSES; WATER; ORGANIZATION;
CONVECTION
AB Effects of vertical wind shear, radiation, and ice clouds on cloud microphysical budget associated with torrential rainfall during landfall of severe tropical storm Bilis (2006) are investigated by using a series of analysis of two-day grid-scale sensitivity experiment data. When upper-tropospheric upward motions and lower-tropospheric downward motions occur on 15 July 2006, the removal of vertical wind shear and ice clouds increases rainfall contributions from the rainfall type (CM) associated with positive net condensation and hydrometeor loss/convergence, whereas the exclusion of cloud radiative effects and cloud-radiation interaction reduces rainfall contribution from CM. The elimination of vertical wind shear and cloud-radiation interaction increases rainfall contribution from the rainfall type (Cm) associated with positive net condensation and hydrometeor gain/divergence, but the removal of cloud radiative effects and ice clouds decreases rainfall contribution from Cm. The enhancements in rainfall contribution from the rainfall type (cM) associated with negative net condensation and hydrometeor loss/convergence are caused by the exclusion of cloud radiative effects, cloud-radiation interaction and ice clouds, whereas the reduction in rainfall contribution from cM results from the removal of vertical wind shear. When upward motions appear throughout the troposphere on 16 July, the exclusion of all these effects increases rainfall contribution from CM, but generally decreases rainfall contributions from Cm and cM.
C1 [Wang Donghai; Liu Ying; Yin Jinfang] Chinese Acad Meteorol Sci, State Key Lab Severe Weather, Beijing 100081, Peoples R China.
[Wang Donghai] Sci Syst & Applicat Inc, Lanham, MD 20706 USA.
[Zhu Ping] Florida Int Univ, Dept Earth & Environm, Miami, FL 33199 USA.
[Li Xiaofan] NOAA, NESDIS, Ctr Satellite Applicat & Res, Camp Springs, MD 20746 USA.
[Tao Wei-Kuo] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Wang, DH (reprint author), Chinese Acad Meteorol Sci, State Key Lab Severe Weather, Beijing 100081, Peoples R China.
EM d.wang@hotmail.com
RI Li, Xiaofan/F-5605-2010; Li, Xiaofan/G-2094-2014
FU National (Key) Basic Research and Development (973) Program of China
[2012CB417204]; China Meteorological Administration [GYHY200806007,
GYHY201006014, GYHY201206039]; National Natural Science Foundation of
China [40875022, 40633016, 41175064]; State Key Laboratory of Severe
Weather, Chinese Academy of Meteorological Sciences
FX Supported by the National (Key) Basic Research and Development (973)
Program of China (2012CB417204), China Meteorological Administration
Special Public Welfare Research Fund (GYHY200806007, GYHY201006014, and
GYHY201206039), National Natural Science Foundation of China (40875022,
40633016, and 41175064), and Basic Research Project of the State Key
Laboratory of Severe Weather, Chinese Academy of Meteorological
Sciences.
NR 26
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PU SPRINGER HEIDELBERG
PI HEIDELBERG
PA TIERGARTENSTRASSE 17, D-69121 HEIDELBERG, GERMANY
SN 0894-0525
J9 ACTA METEOROL SIN
JI Acta Meteorol. Sin.
PD APR
PY 2013
VL 27
IS 2
BP 263
EP 272
DI 10.1007/s13351-013-0210-z
PG 10
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 135PW
UT WOS:000318302000010
ER
PT J
AU McKay, CP
Stoker, CR
Glass, BJ
Dave, AI
Davila, AF
Heldmann, JL
Marinova, MM
Fairen, AG
Quinn, RC
Zacny, KA
Paulsen, G
Smith, PH
Parro, V
Andersen, DT
Hecht, MH
Lacelle, D
Pollard, WH
AF McKay, Christopher P.
Stoker, Carol R.
Glass, Brian J.
Dave, Arwen I.
Davila, Alfonso F.
Heldmann, Jennifer L.
Marinova, Margarita M.
Fairen, Alberto G.
Quinn, Richard C.
Zacny, Kris A.
Paulsen, Gale
Smith, Peter H.
Parro, Victor
Andersen, Dale T.
Hecht, Michael H.
Lacelle, Denis
Pollard, Wayne H.
TI The Icebreaker Life Mission to Mars: A Search for Biomolecular Evidence
for Life
SO ASTROBIOLOGY
LA English
DT Article
DE In situ measurement; Life detection; Mars; Planetary protection; Special
region
ID PHOENIX LANDING SITE; MARTIAN SOIL; MERIDIANI-PLANUM; GROUND ICE;
ORGANIC-COMPOUNDS; LIQUID WATER; SURFACE; PERMAFROST; CARBONATE; IRON
AB The search for evidence of life on Mars is the primary motivation for the exploration of that planet. The results from previous missions, and the Phoenix mission in particular, indicate that the ice-cemented ground in the north polar plains is likely to be the most recently habitable place that is currently known on Mars. The near-surface ice likely provided adequate water activity during periods of high obliquity, similar to 5 Myr ago. Carbon dioxide and nitrogen are present in the atmosphere, and nitrates may be present in the soil. Perchlorate in the soil together with iron in basaltic rock provides a possible energy source for life. Furthermore, the presence of organics must once again be considered, as the results of the Viking GCMS are now suspect given the discovery of the thermally reactive perchlorate. Ground ice may provide a way to preserve organic molecules for extended periods of time, especially organic biomarkers. The Mars Icebreaker Life mission focuses on the following science goals: (1) Search for specific biomolecules that would be conclusive evidence of life. (2) Perform a general search for organic molecules in the ground ice. (3) Determine the processes of ground ice formation and the role of liquid water. (4) Understand the mechanical properties of the martian polar ice-cemented soil. (5) Assess the recent habitability of the environment with respect to required elements to support life, energy sources, and possible toxic elements. (6) Compare the elemental composition of the northern plains with midlatitude sites. The Icebreaker Life payload has been designed around the Phoenix spacecraft and is targeted to a site near the Phoenix landing site. However, the Icebreaker payload could be supported on other Mars landing systems. Preliminary studies of the SpaceX Dragon lander show that it could support the Icebreaker payload for a landing either at the Phoenix site or at midlatitudes. Duplicate samples could be cached as a target for possible return by a Mars Sample Return mission. If the samples were shown to contain organic biomarkers, interest in returning them to Earth would be high.
C1 [McKay, Christopher P.; Stoker, Carol R.; Glass, Brian J.; Dave, Arwen I.; Davila, Alfonso F.; Heldmann, Jennifer L.; Marinova, Margarita M.; Fairen, Alberto G.; Quinn, Richard C.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Zacny, Kris A.; Paulsen, Gale] Honeybee Robot, Pasadena, CA USA.
[Smith, Peter H.] Univ Arizona, Tucson, AZ USA.
[Parro, Victor] Ctr Astrobio INTA CSIC, Madrid, Spain.
[Andersen, Dale T.] SETI Inst, Mountain View, CA USA.
[Hecht, Michael H.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Lacelle, Denis] Univ Ottawa, Ottawa, ON, Canada.
[Pollard, Wayne H.] McGill Univ, Montreal, PQ, Canada.
RP McKay, CP (reprint author), NASA, Ames Res Ctr, Div Space Sci, Moffett Field, CA 94035 USA.
EM chris.mckay@nasa.gov
RI sebastianovitsch, stepan/G-8507-2013;
OI Lacelle, Denis/0000-0002-6691-8717
FU NASA ASTEP program; NASA ASTID program
FX This work was supported by the NASA ASTEP and ASTID programs.
NR 122
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U1 7
U2 106
PU MARY ANN LIEBERT, INC
PI NEW ROCHELLE
PA 140 HUGUENOT STREET, 3RD FL, NEW ROCHELLE, NY 10801 USA
SN 1531-1074
J9 ASTROBIOLOGY
JI Astrobiology
PD APR
PY 2013
VL 13
IS 4
BP 334
EP 353
DI 10.1089/ast.2012.0878
PG 20
WC Astronomy & Astrophysics; Biology; Geosciences, Multidisciplinary
SC Astronomy & Astrophysics; Life Sciences & Biomedicine - Other Topics;
Geology
GA 130ZX
UT WOS:000317961000003
PM 23560417
ER
PT J
AU Dave, A
Thompson, SJ
McKay, CP
Stoker, CR
Zacny, K
Paulsen, G
Mellerowicz, B
Glass, BJ
Willson, D
Bonaccorsi, R
Rask, J
AF Dave, Arwen
Thompson, Sarah J.
McKay, Christopher P.
Stoker, Carol R.
Zacny, Kris
Paulsen, Gale
Mellerowicz, Bolek
Glass, Brian J.
Willson, David
Bonaccorsi, Rosalba
Rask, Jon
TI The Sample Handling System for the Mars Icebreaker Life Mission: From
Dirt to Data
SO ASTROBIOLOGY
LA English
DT Article
DE Mars; Analogue; Life-detection instruments; Planetary protection;
Spacecraft experiments
ID SITE; ANALOG
AB The Mars Icebreaker Life mission will search for subsurface life on Mars. It consists of three payload elements: a drill to retrieve soil samples from approximately 1 m below the surface, a robotic sample handling system to deliver the sample from the drill to the instruments, and the instruments themselves. This paper will discuss the robotic sample handling system.
Collecting samples from ice-rich soils on Mars in search of life presents two challenges: protection of that icy soil-considered a "special region" with respect to planetary protection-from contamination from Earth, and delivery of the icy, sticky soil to spacecraft instruments. We present a sampling device that meets these challenges. We built a prototype system and tested it at martian pressure, drilling into ice-cemented soil, collecting cuttings, and transferring them to the inlet port of the SOLID2 life-detection instrument. The tests successfully demonstrated that the Icebreaker drill, sample handling system, and life-detection instrument can collectively operate in these conditions and produce science data that can be delivered via telemetry-from dirt to data. Our results also demonstrate the feasibility of using an air gap to prevent forward contamination. We define a set of six analog soils for testing over a range of soil cohesion, from loose sand to basalt soil, with angles of repose of 27 degrees and 39 degrees, respectively. Particle size is a key determinant of jamming of mechanical parts by soil particles. Jamming occurs when the clearance between moving parts is equal in size to the most common particle size or equal to three of these particles together. Three particles acting together tend to form bridges and lead to clogging. Our experiments show that rotary-hammer action of the Icebreaker drill influences the particle size, typically reducing particle size by similar to 100 mu m.
C1 [Dave, Arwen; Thompson, Sarah J.; McKay, Christopher P.; Stoker, Carol R.; Glass, Brian J.; Willson, David; Bonaccorsi, Rosalba] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Dave, Arwen] Lockheed Martin IS&GS, Moffett Field, CA USA.
[Thompson, Sarah J.] Stinger Ghaffarian Technol Inc, Moffett Field, CA USA.
[Zacny, Kris; Paulsen, Gale; Mellerowicz, Bolek] Honeybee Robot, Pasadena, CA USA.
[Willson, David] KISS Inst Pract Robot, Moffett Field, CA USA.
[Bonaccorsi, Rosalba] SETI Inst, Mountain View, CA USA.
[Rask, Jon] NASA, Ames Res Ctr, Space Biosci Div, Dynamac Inc, Mountain View, CA USA.
RP Dave, A (reprint author), NASA, Ames Res Ctr, Planetary Syst Branch, MS N240A-4, Moffett Field, CA 94035 USA.
EM arwen.i.dave@nasa.gov
FU NASA ASTEP program; NASA ASTID program; Lockheed Martin ISGS
FX We'd like to thank the members of the extended team that made this
testing and analysis possible. Thanks to the NASA and Lockheed Martin
staff that supported the ambient testing at Ames Research Center: Roger
Arno for his design work, Emmett Quigley for expert help in fabrication
and modification, Ryan Walker for help with microscopic particle size
analysis, and John Livacich for backhoe and contamination control advice
and help with evaluation criteria. Mike Hecht for providing raw data
from Phoenix soil measurements. This project was supported by the NASA
ASTEP and ASTID programs and Lockheed Martin IS&GS.
NR 27
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U1 0
U2 16
PU MARY ANN LIEBERT INC
PI NEW ROCHELLE
PA 140 HUGUENOT STREET, 3RD FL, NEW ROCHELLE, NY 10801 USA
SN 1531-1074
J9 ASTROBIOLOGY
JI Astrobiology
PD APR
PY 2013
VL 13
IS 4
BP 354
EP 369
DI 10.1089/ast.2012.0911
PG 16
WC Astronomy & Astrophysics; Biology; Geosciences, Multidisciplinary
SC Astronomy & Astrophysics; Life Sciences & Biomedicine - Other Topics;
Geology
GA 130ZX
UT WOS:000317961000004
PM 23577818
ER
PT J
AU Kains, N
Street, RA
Choi, JY
Han, C
Udalski, A
Almeida, LA
Jablonski, F
Tristram, PJ
Jorgensen, UG
Szymanski, MK
Kubiak, M
Pietrzynski, G
Soszynski, I
Poleski, R
Kozlowski, S
Pietrukowicz, P
Ulaczyk, K
Wyrzykowski, L
Skowron, J
Alsubai, KA
Bozza, V
Browne, P
Burgdorf, MJ
Novati, SC
Dodds, P
Dominik, M
Dreizler, S
Fang, XS
Grundahl, F
Gu, CH
Hardis, S
Harpsoe, K
Hessman, FV
Hinse, TC
Hornstrup, A
Hundertmark, M
Jessen-Hansen, J
Kerins, E
Liebig, C
Lund, M
Lundkvist, M
Mancini, L
Mathiasen, M
Penny, MT
Rahvar, S
Ricci, D
Sahu, KC
Scarpetta, G
Skottfelt, J
Snodgrass, C
Southworth, J
Surdej, J
Tregloan-Reed, J
Wambsganss, J
Wertz, O
Bajek, D
Bramich, DM
Horne, K
Ipatov, S
Steele, IA
Tsapras, Y
Abe, F
Bennett, DP
Bond, IA
Botzler, CS
Chote, P
Freeman, M
Fukui, A
Furusawa, K
Itow, Y
Ling, CH
Masuda, K
Matsubara, Y
Miyake, N
Muraki, Y
Ohnishi, K
Rattenbury, N
Saito, T
Sullivan, DJ
Sumi, T
Suzuki, D
Suzuki, K
Sweatman, WL
Takino, S
Wada, K
Yock, PCM
Allen, W
Batista, V
Chung, SJ
Christie, G
DePoy, DL
Drummond, J
Gaudi, BS
Gould, A
Henderson, C
Jung, YK
Koo, JR
Lee, CU
McCormick, J
McGregor, D
Munoz, JA
Natusch, T
Ngan, H
Park, H
Pogge, RW
Shin, IG
Yee, J
Albrow, MD
Bachelet, E
Beaulieu, JP
Brillant, S
Caldwell, JAR
Cassan, A
Cole, A
Corrales, E
Coutures, C
Dieters, S
Prester, DD
Donatowicz, J
Fouque, P
Greenhill, J
Kane, SR
Kubas, D
Marquette, JB
Martin, R
Meintjes, P
Menzies, J
Pollard, KR
Williams, A
Wouters, D
Zub, A
AF Kains, N.
Street, R. A.
Choi, J. -Y.
Han, C.
Udalski, A.
Almeida, L. A.
Jablonski, F.
Tristram, P. J.
Jorgensen, U. G.
Szymanski, M. K.
Kubiak, M.
Pietrzynski, G.
Soszynski, I.
Poleski, R.
Kozlowski, S.
Pietrukowicz, P.
Ulaczyk, K.
Wyrzykowski, L.
Skowron, J.
Alsubai, K. A.
Bozza, V.
Browne, P.
Burgdorf, M. J.
Novati, S. Calchi
Dodds, P.
Dominik, M.
Dreizler, S.
Fang, X. -S.
Grundahl, F.
Gu, C-H.
Hardis, S.
Harpsoe, K.
Hessman, F. V.
Hinse, T. C.
Hornstrup, A.
Hundertmark, M.
Jessen-Hansen, J.
Kerins, E.
Liebig, C.
Lund, M.
Lundkvist, M.
Mancini, L.
Mathiasen, M.
Penny, M. T.
Rahvar, S.
Ricci, D.
Sahu, K. C.
Scarpetta, G.
Skottfelt, J.
Snodgrass, C.
Southworth, J.
Surdej, J.
Tregloan-Reed, J.
Wambsganss, J.
Wertz, O.
Bajek, D.
Bramich, D. M.
Horne, K.
Ipatov, S.
Steele, I. A.
Tsapras, Y.
Abe, F.
Bennett, D. P.
Bond, I. A.
Botzler, C. S.
Chote, P.
Freeman, M.
Fukui, A.
Furusawa, K.
Itow, Y.
Ling, C. H.
Masuda, K.
Matsubara, Y.
Miyake, N.
Muraki, Y.
Ohnishi, K.
Rattenbury, N.
Saito, T.
Sullivan, D. J.
Sumi, T.
Suzuki, D.
Suzuki, K.
Sweatman, W. L.
Takino, S.
Wada, K.
Yock, P. C. M.
Allen, W.
Batista, V.
Chung, S. -J.
Christie, G.
DePoy, D. L.
Drummond, J.
Gaudi, B. S.
Gould, A.
Henderson, C.
Jung, Y. -K.
Koo, J. -R.
Lee, C. -U.
McCormick, J.
McGregor, D.
Munoz, J. A.
Natusch, T.
Ngan, H.
Park, H.
Pogge, R. W.
Shin, I. -G.
Yee, J.
Albrow, M. D.
Bachelet, E.
Beaulieu, J. -P.
Brillant, S.
Caldwell, J. A. R.
Cassan, A.
Cole, A.
Corrales, E.
Coutures, Ch.
Dieters, S.
Prester, D. Dominis
Donatowicz, J.
Fouque, P.
Greenhill, J.
Kane, S. R.
Kubas, D.
Marquette, J. -B.
Martin, R.
Meintjes, P.
Menzies, J.
Pollard, K. R.
Williams, A.
Wouters, D.
Zub, Andm.
CA OGLE Collaboration
MiNDSTEp Consortium
RoboNet Collaboration
MOA Collaboration
FUN Collaboration
PLANET Collaboration
TI A giant planet beyond the snow line in microlensing event
OGLE-2011-BLG-0251
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE gravitational lensing: weak; planets and satellites: detection;
planetary systems; Galaxy: bulge
ID BINARY; DWARF; MASS; LENS; STARS; ALGORITHM; DISCOVERY; FREQUENCY;
SYSTEMS; SEARCH
AB Aims. We present the analysis of the gravitational microlensing event OGLE-2011-BLG-0251. This anomalous event was observed by several survey and follow-up collaborations conducting microlensing observations towards the Galactic bulge.
Methods. Based on detailed modelling of the observed light curve, we find that the lens is composed of two masses with a mass ratio q = 1.9 x 10(-3). Thanks to our detection of higher-order effects on the light curve due to the Earth's orbital motion and the finite size of source, we are able to measure the mass and distance to the lens unambiguously.
Results. We find that the lens is made up of a planet of mass 0.53 +/- 0.21 M-J orbiting an M dwarf host star with a mass of 0.26 +/- 0.11 M-circle dot. The planetary system is located at a distance of 2.57 +/- 0.61 kpc towards the Galactic centre. The projected separation of the planet from its host star is d = 1.408 +/- 0.019, in units of the Einstein radius, which corresponds to 2.72 +/- 0.75 AU in physical units. We also identified a competitive model with similar planet and host star masses, but with a smaller orbital radius of 1.50 +/- 0.50 AU. The planet is therefore located beyond the snow line of its host star, which we estimate to be around similar to 1-1.5 AU.
C1 [Kains, N.; Bramich, D. M.] European So Observ, D-85748 Garching, Germany.
[Street, R. A.; Tsapras, Y.] Las Cumbres Observ Global Telescope Network, Goleta, CA 93117 USA.
[Choi, J. -Y.; Han, C.; Jung, Y. -K.; Park, H.; Shin, I. -G.] Chungbuk Natl Univ, Inst Astrophys, Dept Phys, Chonju 371763, South Korea.
[Udalski, A.; Szymanski, M. K.; Kubiak, M.; Pietrzynski, G.; Soszynski, I.; Poleski, R.; Kozlowski, S.; Pietrukowicz, P.; Ulaczyk, K.; Wyrzykowski, L.; Skowron, J.] Univ Warsaw Observ, PL-00478 Warsaw, Poland.
[Almeida, L. A.; Jablonski, F.] Inst Nacl Pesquisas Espaciais, Div Astrofis, BR-12227010 Sao Jose Dos Campos, SP, Brazil.
[Tristram, P. J.; Chote, P.; Sullivan, D. J.] Victoria Univ, Sch Chem & Phys Sci, Wellington, New Zealand.
[Jorgensen, U. G.; Hardis, S.; Harpsoe, K.; Hinse, T. C.; Mathiasen, M.; Skottfelt, J.] Univ Copenhagen, Niels Bohr Inst, DK-2100 Copenhagen, Denmark.
[Jorgensen, U. G.; Harpsoe, K.] Geol Museum, Ctr Star & Planet Format, DK-1350 Copenhagen, Denmark.
[Alsubai, K. A.] Qatar Fdn, Doha, Qatar.
[Bozza, V.; Novati, S. Calchi; Scarpetta, G.] Univ Salerno, Dipartimento Fis ER Caianiello, I-84084 Fisciano, Italy.
[Bozza, V.] Ist Nazl Fis Nucl, Sez Napoli, Naples, Italy.
[Browne, P.; Dodds, P.; Dominik, M.; Hundertmark, M.; Liebig, C.; Bajek, D.; Horne, K.] Univ St Andrews, SUPA Sch Phys & Astron, St Andrews KY16 9SS, Fife, Scotland.
[Burgdorf, M. J.] Univ Stuttgart, Deutsch SOFIA Inst, D-70569 Stuttgart, Germany.
[Burgdorf, M. J.] NASA, Ames Res Ctr, SOFIA Sci Ctr, Moffett Field, CA 94035 USA.
[Novati, S. Calchi] IIASS, Vietri Sul Mare, SA, Italy.
[Dreizler, S.; Hessman, F. V.; Hundertmark, M.] Univ Gottingen, Inst Astrophys, D-37077 Gottingen, Germany.
[Hinse, T. C.; Chung, S. -J.; Koo, J. -R.; Lee, C. -U.] Korea Astron & Space Sci Inst, Taejon 305348, South Korea.
[Fang, X. -S.; Gu, C-H.] Chinese Acad Sci, Yunnan Observ, Natl Astron Observ, Joint Lab Opt Astron, Kunming 650011, Peoples R China.
[Grundahl, F.; Jessen-Hansen, J.; Lund, M.; Lundkvist, M.] Aarhus Univ, Dept Phys & Astron, DK-8000 Aarhus C, Denmark.
[Hinse, T. C.] Armagh Observ, Armagh BT61 9DG, North Ireland.
Danmarks Tekniske Univ, Inst Rumforskning Og Teknol, DK-2100 Copenhagen, Denmark.
[Hornstrup, A.; Kerins, E.; Penny, M. T.] Univ Manchester, Jodrell Bank Ctr Astrophys, Oxford M13 9PL, England.
[Mancini, L.] Max Planck Inst Astron, D-69117 Heidelberg, Germany.
[Poleski, R.; Skowron, J.; Penny, M. T.; Batista, V.; Gaudi, B. S.; Gould, A.; Henderson, C.; McGregor, D.; Pogge, R. W.; Yee, J.] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA.
[Rahvar, S.] Sharif Univ Technol, Dept Phys, Tehran, Iran.
[Rahvar, S.] Perimeter Inst Theoret Phys, Waterloo, ON N2L 2Y5, Canada.
[Ricci, D.; Surdej, J.; Wertz, O.] Inst Astrophys & Geophys, B-4000 Liege, Belgium.
[Sahu, K. C.] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
[Scarpetta, G.] Ist Nazl Fis Nucl, Grp Collegato Salerno, Sez Napoli, Naples, Italy.
[Brillant, S.; Kubas, D.] ESO, Santiago 19, Chile.
[Snodgrass, C.] Max Planck Inst Solar Syst Res, D-37191 Katlenburg Lindau, Germany.
[Southworth, J.; Tregloan-Reed, J.] Keele Univ, Astrophys Grp, Keele ST5 5BG, Staffs, England.
[Wambsganss, J.; Williams, A.; Zub, Andm.] Univ Heidelberg ZAH, Zentrum Astron, Astron Rechen Inst, D-69120 Heidelberg, Germany.
[Wyrzykowski, L.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England.
[Ipatov, S.] Alsubais Estab Sci Studies, Doha, Qatar.
[Steele, I. A.] Liverpool John Moores Univ, Astrophys Res Inst, Birkenhead CH41 1LD, Wirral, England.
[Tsapras, Y.] Univ London, Sch Math Sci, London E1 4NS, England.
[Allen, W.] Vintage Lane Observ, Blenheim, New Zealand.
[Christie, G.; Natusch, T.; Ngan, H.] Auckland Observ, Auckland 1023, New Zealand.
[DePoy, D. L.] Texas A&M Univ, Dept Phys & Astron, College Stn, TX 77843 USA.
[Drummond, J.] Possum Observ, Patutahi, Gisbourne, New Zealand.
[McCormick, J.] Ctr Backyard Astrophys, Farm Cove Observ, Auckland, New Zealand.
[Natusch, T.] AUT Univ, Inst Radiophys & Space Res, Auckland, New Zealand.
Chungnam Natl Univ, Dept Astron & Space Sci, Oneonta, NY USA.
[Munoz, J. A.] Univ Valencia, Dept Astron & Astrofis, E-46100 Valencia, Spain.
[Beaulieu, J. -P.; Cassan, A.; Corrales, E.; Coutures, Ch.; Kubas, D.; Marquette, J. -B.; Wouters, D.] UPMC CNRS, UMR7095, Inst Astrophys Paris, F-75014 Paris, France.
[Albrow, M. D.; Pollard, K. R.] Univ Canterbury, Dept Phys & Astron, Christchurch 8020, New Zealand.
[Caldwell, J. A. R.] McDonald Observ, Ft Davis, TX 79734 USA.
[Meintjes, P.] Univ Free State, Fac Nat & Agr Sci, Dept Phys, ZA-9300 Bloemfontein, South Africa.
[Cole, A.; Greenhill, J.] Univ Tasmania, Sch Math & Phys, Gpo Hobart, Tas 7001, Australia.
Lawrence Livermore Natl Lab, IGPP, Livermore, CA 94551 USA.
[Bachelet, E.; Dieters, S.; Fouque, P.] Univ Toulouse, UPS OMP, IRAP, F-31400 Toulouse, France.
[Bachelet, E.; Fouque, P.] CNRS, IRAP, F-31400 Toulouse, France.
[Prester, D. Dominis] Univ Rijeka, Fac Arts & Sci, Dept Phys, Rijeka 51000, Croatia.
[Donatowicz, J.] Vienna Univ Technol, Dept Comp, A-1060 Vienna, Austria.
[Kane, S. R.] CALTECH, NASA Exoplanet Sci Inst, Pasadena, CA 91125 USA.
[Martin, R.] Perth Observ, Perth, WA 6076, Australia.
[Menzies, J.] S African Astron Observ, ZA-7935 Observatory, South Africa.
[Abe, F.; Furusawa, K.; Itow, Y.; Masuda, K.; Matsubara, Y.; Miyake, N.; Suzuki, K.; Takino, S.] Nagoya Univ, Solar Terr Environm Lab, Nagoya, Aichi 4648601, Japan.
[Bennett, D. P.] Univ Notre Dame, Dept Phys, Notre Dame, IN 46556 USA.
[Bond, I. A.; Ling, C. H.; Sweatman, W. L.] Massey Univ, Inst Informat & Math Sci, North Shore Mail Ctr, Auckland, New Zealand.
[Botzler, C. S.; Freeman, M.; Rattenbury, N.; Yock, P. C. M.] Univ Auckland, Dept Phys, Auckland, New Zealand.
[Fukui, A.] Natl Astron Observ Japan, Okayama Astrophys Observ, Okayama 7190232, Japan.
Mt John Observ, Lake Tekapo 8770, New Zealand.
[Muraki, Y.] Konan Univ, Dept Phys, Kobe, Hyogo 6588501, Japan.
[Ohnishi, K.] Nagano Natl Coll Technol, Nagano 3818550, Japan.
[Saito, T.] Tokyo Metropolitan Coll Ind Technol, Tokyo 1168523, Japan.
[Sumi, T.; Suzuki, D.; Wada, K.] Osaka Univ, Grad Sch Sci, Dept Earth & Space Sci, Toyonaka, Osaka 5600043, Japan.
[Pietrzynski, G.] Univ Concepcion, Dept Astron, Concepcion, Chile.
RP Kains, N (reprint author), European So Observ, Karl Schwarzschild Str 2, D-85748 Garching, Germany.
EM nkains@eso.org; cheongho@astroph.chungbuk.ac.kr
RI Almeida, L./G-7188-2012; Kozlowski, Szymon/G-4799-2013; Williams,
Andrew/K-2931-2013; Skowron, Jan/M-5186-2014; Hundertmark,
Markus/C-6190-2015; Rahvar, Sohrab/A-9350-2008; Ipatov,
Sergei/O-2302-2014
OI Ricci, Davide/0000-0002-9790-0552; Penny, Matthew/0000-0001-7506-5640;
Snodgrass, Colin/0000-0001-9328-2905; Lund, Mikkel
Norup/0000-0001-9214-5642; Lundkvist, Mia Sloth/0000-0002-8661-2571;
Cole, Andrew/0000-0003-0303-3855; Kozlowski, Szymon/0000-0003-4084-880X;
Williams, Andrew/0000-0001-9080-0105; Skowron, Jan/0000-0002-2335-1730;
Hundertmark, Markus/0000-0003-0961-5231; Rahvar,
Sohrab/0000-0002-7084-5725; Dominik, Martin/0000-0002-3202-0343; Ipatov,
Sergei/0000-0002-1413-9180
FU ESO; European Community [229517, 268421]; European Research Council
under the European Community [246678]; NPRP from the Qatar National
Research Fund (a member of Qatar Foundation) [NPRP-09-476-1-78];
Creative Research Initiative Program of National Research Foundation of
Korea [2009-0081561]; Danish Natural Science Foundation (FNU); German
Research Foundation (DFG); Communaute francaise de Belgique - Actions de
recherche concertees - Academie universitaire Wallonie-Europe; Korea
Research Council for Fundamental Science and Technology (KRCF); KASI
(Korea Astronomy and Space Science Institute) [2012-1-410-02]; National
Science Foundation Graduate Research Fellowship [2009068160]; NSF; NASA
[NNX12AB99G]; JSPS [JSPS23540339, JSPS19340058]; [JSPS22403003];
[JSPS23340064]; [JSPS23340044]
FX N.K. acknowledges an ESO Fellowship. The research leading to these
results has received funding from the European Community's Seventh
Framework Programme (/FP7/2007-2013/) under grant agreements No 229517
and 268421. The OGLE project has received funding from the European
Research Council under the European Community's Seventh Framework
Programme (FP7/2007-2013) / ERC grant agreement No. 246678 to AU. K. A.,
D. B., M. D., K. H., M. H., S. I., C. L., R. S., Y.T. are supported by
NPRP grant NPRP-09-476-1-78 from the Qatar National Research Fund (a
member of Qatar Foundation). Work by C. Han was supported by Creative
Research Initiative Program (2009-0081561) of National Research
Foundation of Korea. This work is based in part on data collected by
MiNDSTEp with the Danish 1.54 m telescope at the ESO La Silla
Observatory. The Danish 1.54 m telescope is operated based on a grant
from the Danish Natural Science Foundation (FNU). The MiNDSTEp
monitoring campaign is powered by ARTEMiS (Automated Terrestrial
Exoplanet Microlensing Search; Dominik et al. 2008). M. H. acknowledges
support by the German Research Foundation (DFG). D. R. (boursier FRIA),
O.W. (aspirant FRS - FNRS) and J. Surdej acknowledge support from the
Communaute francaise de Belgique - Actions de recherche concertees -
Academie universitaire Wallonie-Europe. T. C. H. gratefully acknowledges
financial support from the Korea Research Council for Fundamental
Science and Technology (KRCF) through the Young Research Scientist
Fellowship Program. T. C. H. and C. U. L. acknowledge financial support
from KASI (Korea Astronomy and Space Science Institute) grant number
2012-1-410-02. Work by J. C. Yee is supported by a National Science
Foundation Graduate Research Fellowship under Grant No. 2009068160. A.
Gould and B. S. Gaudi acknowledge support from NSF AST-1103471. B. S.
Gaudi, A. Gould, and R. W. Pogge acknowledge support from NASA grant
NNX12AB99G. The MOA experiment was supported by grants JSPS22403003 and
JSPS23340064. T. S. was supported by the grant JSPS23340044. Y. Muraki
acknowledges support from JSPS grants JSPS23540339 and JSPS19340058.
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JI Astron. Astrophys.
PD APR
PY 2013
VL 552
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PG 10
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SC Astronomy & Astrophysics
GA 130JW
UT WOS:000317912000070
ER
PT J
AU Kuulkers, E
Kouveliotou, C
Belloni, T
Bel, MC
Chenevez, J
Trigo, MD
Homan, J
Ibarra, A
Kennea, JA
Munoz-Darias, T
Ness, JU
Parmar, AN
Pollock, AMT
van den Heuvel, EPJ
van der Horst, AJ
AF Kuulkers, E.
Kouveliotou, C.
Belloni, T.
Cadolle Bel, M.
Chenevez, J.
Trigo, M. Diaz
Homan, J.
Ibarra, A.
Kennea, J. A.
Munoz-Darias, T.
Ness, J. -U.
Parmar, A. N.
Pollock, A. M. T.
van den Heuvel, E. P. J.
van der Horst, A. J.
TI MAXI J1659-152: the shortest orbital period black-hole transient in
outburst
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE accretion, accretion disks; binaries: close; stars: individual: MAXI
J1659-152; X-rays: binaries
ID X-RAY BINARIES; DRIVEN ECCENTRIC INSTABILITIES; ACCRETING COMPACT
OBJECTS; PHOTON IMAGING CAMERA; BOARD XMM-NEWTON; LOW-MASS; CATACLYSMIC
VARIABLES; SWIFT J1753.5-0127; LIGHT CURVES; CYGNUS X-1
AB MAXI J1659-152 is a bright X-ray transient black-hole candidate binary system discovered in September 2010. We report here on MAXI, RXTE, Swift, and XMM-Newton observations during its 2010/2011 outburst. We find that during the first one and a half week of the outburst the X-ray light curves display drops in intensity at regular intervals, which we interpret as absorption dips. About three weeks into the outbursts, again drops in intensity are seen. These dips have, however, a spectral behaviour opposite to that of the absorption dips, and are related to fast spectral state changes (hence referred to as transition dips). The absorption dips recur with a period of 2.414 +/- 0.005 h, which we interpret as the orbital period of the system. This implies that MAXI J1659-152 is the shortest period black-hole candidate binary known to date. The inclination of the accretion disk with respect to the line of sight is estimated to be 65-80 degrees. We propose the companion to the black-hole candidate to be close to an M5 dwarf star, with a mass and radius of about 0.15-0.25 M-circle dot and 0.2-0.25 R-circle dot, respectively. We derive that the companion had an initial mass of about 1.5 M-circle dot, which evolved to its current mass in about 5-6 billion years. The system is rather compact (orbital separation of greater than or similar to 1.33 R-circle dot), and is located at a distance of 8.6 +/- 3.7 kpc, with a height above the Galactic plane of 2.4 +/- 1.0 kpc. The characteristics of short orbital period and high Galactic scale height are shared with two other transient black-hole candidate X-ray binaries, i.e., XTE J1118+480 and Swift J1735.5-0127. We suggest that all three are kicked out of the Galactic plane into the halo, rather than being formed in a globular cluster.
C1 [Kuulkers, E.; Cadolle Bel, M.; Ibarra, A.; Ness, J. -U.; Parmar, A. N.; Pollock, A. M. T.] European Space Astron Ctr ESA ESAC, Sci Operat Dept, Madrid 28691, Spain.
[Kouveliotou, C.] NASA, Astrophys Off, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA.
[Belloni, T.; Munoz-Darias, T.] INAF Osservatorio Astron Brera, I-23807 Merate, LC, Italy.
[Chenevez, J.] Tech Univ Denmark, Natl Space Inst, DK-2800 Lyngby, Denmark.
[Trigo, M. Diaz] ESO, D-85748 Garching, Germany.
[Homan, J.] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA.
[Kennea, J. A.] Penn State Univ, Dept Astron & Astrophys, Davey Lab 525, University Pk, PA 16802 USA.
[Munoz-Darias, T.] Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England.
[van den Heuvel, E. P. J.; van der Horst, A. J.] Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1098 XH Amsterdam, Netherlands.
[van der Horst, A. J.] NSSTC, Univ Space Res Assoc, Huntsville, AL 35805 USA.
RP Kuulkers, E (reprint author), European Space Astron Ctr ESA ESAC, Sci Operat Dept, Madrid 28691, Spain.
EM Erik.Kuulkers@esa.int
OI Parmar, Arvind/0000-0002-3307-6517
FU ESA Member States; NASA; European Community's Seventh Framework
Programme [ITN 215212]; EU Marie Curie Intra-European Fellowship
[2011-301355]; ESA-PRODEX [90057]; [I/009/10/0]
FX Partly based on observations obtained with XMM-Newton, an ESA science
mission with instruments and contributions directly funded by ESA Member
States and NASA. This research has made use of data obtained through the
High Energy Astrophysics Science Archive Research Center Online Service,
provided by the NASA/Goddard Space Flight Center. The MAXI/GSC data are
provided by RIKEN, JAXA and the MAXI team, whilst the Swift/BAT
transient monitor results are provided by the Swift/BAT team. We
especially thank the XMM-Newton Science Operations Centre for their
prompt scheduling of the Target of Opportunity observations, 5 h between
trigger and start of observation on September 27! We would also like to
thank the Swift and RXTE teams for their scheduling of the many
monitoring observations. The research leading to these results has
received funding from the European Community's Seventh Framework
Programme (FP7/2007/2013) under grant agreement number ITN 215212 "Black
Hole Universe". TMB acknowledges support to ASI-INAF grant I/009/10/0,
as well as funding via an EU Marie Curie Intra-European Fellowship under
contract no. 2011-301355. EK thanks John Tonry for discussions regarding
the Pan-STARRS 1 optical candidate, Vik Dhillon for supplying the
"PERIOD" analysis package, which we used in our periodicity analysis,
and Kazutaka Yamaoka for providing the estimated 3-200 keV fluxes from
RXTE spectral fits. E.K. and T.M.D. acknowledge Sara Motta for her
comments on the RXTE spectral analysis. E.K. and M.D.T. thank Roberto
Vio for a discussion on the periodograms. J.C. was supported by
ESA-PRODEX contract N: 90057. Last but not least, we thank the referee
for his/her careful reading of the manuscript.
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JI Astron. Astrophys.
PD APR
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SC Astronomy & Astrophysics
GA 130JW
UT WOS:000317912000032
ER
PT J
AU Olofsson, J
Benisty, M
Le Bouquin, JB
Berger, JP
Lacour, S
Menard, F
Henning, T
Crida, A
Burtscher, L
Meeus, G
Ratzka, T
Pinte, C
Augereau, JC
Malbet, F
Lazareff, B
Traub, W
AF Olofsson, J.
Benisty, M.
Le Bouquin, J. -B.
Berger, J. -P.
Lacour, S.
Menard, F.
Henning, Th
Crida, A.
Burtscher, L.
Meeus, G.
Ratzka, T.
Pinte, C.
Augereau, J. -C.
Malbet, F.
Lazareff, B.
Traub, W.
TI Sculpting the disk around T Chamaeleontis: an interferometric view
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE stars: individual: T Cha; circumstellar matter; infrared: stars;
techniques: interferometric
ID HERBIG AE/BE STARS; PROTOPLANETARY DISKS; RADIATIVE-TRANSFER;
OPTICAL-PROPERTIES; SCATTERED-LIGHT; YOUNG STARS; HD 142527; TAURI;
MODELS; DUST
AB Context. Circumstellar disks are believed to be the birthplace of planets and are expected to dissipate on a timescale of a few Myr. The processes responsible for the removal of the dust and gas will strongly modify the radial distribution of the circumstellar matter and consequently the spectral energy distribution. In particular, a young planet will open a gap, resulting in an inner disk dominating the near-IR emission and an outer disk emitting mostly in the far-infrared.
Aims. We analyze a full set of data involving new near-infrared data obtained with the 4-telescope combiner (VLTI/PIONIER), new mid-infrared interferometric VLTI/MIDI data, literature photometric and archival data from VLT/NaCo/SAM to constrain the structure of the transition disk around T Cha.
Methods. After a preliminary analysis with a simple geometric model, we used the MCFOST radiative transfer code to simultaneously model the SED and the interferometric observables from raytraced images in the H-, L'-, and N-bands.
Results. We find that the dust responsible for the strong emission in excess in the near-IR must have a narrow temperature distribution with a maximum close to the silicate sublimation temperature. This translates into a narrow inner dusty disk (0.07-0.11 AU), with a significant height (H/r similar to 0.2) to increase the geometric surface illuminated by the central star. We find that the outer disk starts at about 12 AU and is partially resolved by the PIONIER, SAM, and MIDI instruments. We discuss the possibility of a self-shadowed inner disk, which can extend to distances of several AU. Finally, we show that the SAM closure phases, interpreted as the signature of a candidate companion, may actually trace the asymmetry generated by forward scattering by dust grains in the upper layers of the outer disk. These observations help constrain the inclination and position angle of the disk to about +58 degrees and -70 degrees, respectively.
Conclusions. The circumstellar environment of T Cha appears to be best described by two disks spatially separated by a large gap. The presence of matter (dust or gas) inside the gap is, however, difficult to assess with present-day observations. Our model suggests the outer disk contaminates the interferometric signature of any potential companion that could be responsible for the gap opening, and such a companion still has to be unambiguously detected. We stress the difficulty to observe point sources in bright massive disks, and the consequent need to account for disk asymmetries (e.g. anisotropic scattering) in model-dependent search for companions.
C1 [Olofsson, J.; Henning, Th] Max Planck Inst Astron, D-69117 Heidelberg, Germany.
[Benisty, M.; Le Bouquin, J. -B.; Menard, F.; Pinte, C.; Augereau, J. -C.; Malbet, F.; Lazareff, B.] UJF Grenoble 1 CNRS INSU, Inst Planetol & Astrophys Grenoble IPAG UMR 5274, Grenoble, France.
[Berger, J. -P.] European So Observ, Alonso De Cordova 3107, Vitacura, Chile.
[Lacour, S.] Univ Paris Diderot, Univ Paris 06, CNRS, LESIA Observ Paris, F-92195 Meudon, France.
[Menard, F.] Univ Chile, CNRS INSU France UMI 3386, UMI FCA, Santiago, Chile.
[Menard, F.] Univ Chile, Dept Astron, Santiago, Chile.
[Crida, A.] Univ Nice Sophia Antipolis CNRS Observ Cote dAzur, Lab Lagrange UMR 7293, F-06304 Nice 04, France.
[Burtscher, L.] Max Planck Inst Extraterr Phys, D-85741 Garching, Germany.
[Meeus, G.] Univ Autonoma Madrid, Dpt Fis Teor, E-28049 Madrid, Spain.
[Ratzka, T.] Univ Munich, Univ Sternwarte Munchen, D-81679 Munich, Germany.
[Traub, W.] Jet Prop Lab NASA JPL, Pasadena, CA 91109 USA.
RP Olofsson, J (reprint author), Max Planck Inst Astron, Konigstuhl 17, D-69117 Heidelberg, Germany.
EM olofsson@mpia.de
OI Ratzka, Thorsten/0000-0001-9557-8232
FU European Commission [PERG06-GA-2009-256513]; Agence Nationale pour la
Recherche (ANR) of France [ANR-2010-JCJC-0504-01]; [089.C-0537(A)]
FX The authors are grateful to the anonymous referee for useful advices and
comments that improved the readability of the paper. The authors thank
Bertram Bitsch for valuable discussions. C.P. acknowledges funding from
the European Commission's 7th Framework Program (contract
PERG06-GA-2009-256513) and from Agence Nationale pour la Recherche (ANR)
of France under contract ANR-2010-JCJC-0504-01. CNRS is acknowledged for
having supported this work in the form of Guaranteed Time Observations
(program 089.C-0537(A)).
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J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD APR
PY 2013
VL 552
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SC Astronomy & Astrophysics
GA 130JW
UT WOS:000317912000004
ER
PT J
AU Sanchez-Monge, A
Cesaroni, R
Beltran, MT
Kumar, MSN
Stanke, T
Zinnecker, H
Etoka, S
Galli, D
Hummel, CA
Moscadelli, L
Preibisch, T
Ratzka, T
van der Tak, FFS
Vig, S
Walmsley, CM
Wang, KS
AF Sanchez-Monge, A.
Cesaroni, R.
Beltran, M. T.
Kumar, M. S. N.
Stanke, T.
Zinnecker, H.
Etoka, S.
Galli, D.
Hummel, C. A.
Moscadelli, L.
Preibisch, T.
Ratzka, T.
van der Tak, F. F. S.
Vig, S.
Walmsley, C. M.
Wang, K. -S.
TI A candidate circumbinary Keplerian disk in G35.20-0.74N: A study with
ALMA
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE stars: formation; ISM: individual objects: G35.20-0.74N; ISM: jets and
outflows
ID YOUNG STELLAR OBJECTS; MOLECULAR OUTFLOWS; IRAS 20126+4104;
STAR-FORMATION; ACCRETION; REGIONS; JET; G35.2-0.74N; AFGL-5142; CLUSTER
AB We report on ALMA observations of continuum and molecular line emission with 0 ''.4 resolution towards the high-mass star-forming region G35.20-0.74 N. Two dense cores are detected in typical hot-core tracers (e. g., CH3CN) that reveal velocity gradients. In one of these cores, the velocity field can be fitted with an almost edge-on Keplerian disk rotating about a central mass of similar to 18 M-circle dot. This finding is consistent with the results of a recent study of the CO first overtone bandhead emission at 2.3 mu m towards G35.20-0.74 N. The disk radius and mass are greater than or similar to 2500 au and similar to 3 M-circle dot. To reconcile the observed bolometric luminosity (similar to 3x10(4) L-circle dot) with the estimated stellar mass of 18 M-circle dot, we propose that the latter is the total mass of a binary system.
C1 [Sanchez-Monge, A.; Cesaroni, R.; Beltran, M. T.; Galli, D.; Moscadelli, L.; Walmsley, C. M.] Osserv Astrofis Arcetri, INAF, I-50125 Florence, Italy.
[Kumar, M. S. N.] Univ Porto, Ctr Astrofis, P-4150762 Oporto, Portugal.
[Stanke, T.; Hummel, C. A.] ESO, D-85748 Garching, Germany.
[Zinnecker, H.] NASA Ames Res Ctr, SOFIA Sci Ctr, Moffett Field, CA 94035 USA.
[Etoka, S.] Univ Manchester, Sch Phys & Astron, Ctr Astrophys, Jodrell Bank, Manchester M13 9PL, Lancs, England.
[Etoka, S.] Hamburger Sternwarte, D-21029 Hamburg, Germany.
[Preibisch, T.; Ratzka, T.] Univ Munich, Univ Sternwarte Munchen, D-81679 Munich, Germany.
[van der Tak, F. F. S.] SRON Netherlands Inst Space Res, NL-9700 AV Groningen, Netherlands.
[van der Tak, F. F. S.] Univ Groningen, Kapteyn Astron Inst, NL-9700 AV Groningen, Netherlands.
[Vig, S.] Indian Inst Space Sci & Technol, Dept Earth & Space Sci, Thiruvananthapuram 695547, Kerala, India.
[Walmsley, C. M.] Dublin Inst Adv Studies DIAS, Dublin 2, Ireland.
[Wang, K. -S.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands.
RP Sanchez-Monge, A (reprint author), Osserv Astrofis Arcetri, INAF, Largo E Fermi 5, I-50125 Florence, Italy.
EM asanchez@arcetri.astro.it
RI Kumar, Nanda/I-4183-2013;
OI Moscadelli, Luca/0000-0002-8517-8881; Galli,
Daniele/0000-0001-7706-6049; Beltran Sorolla, Maria
Teresa/0000-0003-3315-5626; Ratzka, Thorsten/0000-0001-9557-8232;
Cesaroni, Riccardo/0000-0002-2430-5103
FU European ALMA Regional Center; Italian ARC node; NASA; FCT (Portugal);
POPH/FSE (EC)
FX It is a pleasure to thank Goran Sandell for stimulating discussions of
the G35.20-0.74 N region and the anonymous referee for constructive
criticisms. We also acknowledge the support of the European ALMA
Regional Center and the Italian ARC node. This paper makes use of the
following ALMA data: ADS/JAO. ALMA#2011.0.00275. S. ALMA is a
partnership of ESO (representing its member states), NSF (USA), and NINS
(Japan), together with NRC (Canada) and NSC and ASIAA (Taiwan), in
cooperation with the Republic of Chile. The Joint ALMA Observatory is
operated by ESO, AUI/NRAO, and NAOJ. This work also used observations
made with the Spitzer Space Telescope, which is operated by the Jet
Propulsion Laboratory, California Institute of Technology, under a
contract with NASA. MSNK is supported by a Ciencia 2007 contract, funded
by FCT (Portugal) and POPH/FSE (EC).
NR 32
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U1 1
U2 2
PU EDP SCIENCES S A
PI LES ULIS CEDEX A
PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A,
FRANCE
SN 0004-6361
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD APR
PY 2013
VL 552
AR L10
DI 10.1051/0004-6361/201321134
PG 5
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 130JW
UT WOS:000317912000154
ER
PT J
AU Zwintz, K
Fossati, L
Guenther, DB
Ryabchikova, T
Baglin, A
Themessl, N
Barnes, TG
Matthews, JM
Auvergne, M
Bohlender, D
Chaintreuil, S
Kuschnig, R
Moffat, AFJ
Rowe, JF
Rucinski, SM
Sasselov, D
Weiss, WW
AF Zwintz, K.
Fossati, L.
Guenther, D. B.
Ryabchikova, T.
Baglin, A.
Themessl, N.
Barnes, T. G.
Matthews, J. M.
Auvergne, M.
Bohlender, D.
Chaintreuil, S.
Kuschnig, R.
Moffat, A. F. J.
Rowe, J. F.
Rucinski, S. M.
Sasselov, D.
Weiss, W. W.
TI Regular frequency patterns in the young delta Scuti star HD 261711
observed by the CoRoT and MOST satellites
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE stars: variables: delta Scuti; stars: oscillations; stars: individual:
HD261711; techniques: photometric; techniques: spectroscopic
ID PRE-MAIN-SEQUENCE; CLUSTER NGC 2264; LINE-DATA-BASE; DIFFERENTIAL
ROTATION; MODEL ATMOSPHERES; STELLAR EVOLUTION; PRAESEPE CLUSTER;
F-STARS; PHOTOMETRY; SPACE
AB Context. The internal structure of pre-main-sequence (PMS) stars is poorly constrained at present. This could change significantly through high-quality asteroseismological observations of a sample of such stars.
Aims. We concentrate on an asteroseismological study of HD261711, a rather hot delta Scuti-type pulsating member of the young open cluster NGC 2264 located at the blue border of the instability region. HD261711 was discovered to be a PMS delta Scuti star using the time series photometry obtained by the MOST satellite in 2006.
Methods. High-precision, time-series photometry of HD261711 was obtained by the MOST and CoRoT satellites in four separate new observing runs that are put into context with the star's fundamental atmospheric parameters obtained from spectroscopy. Frequency Analysis was performed using Period04. The spectral analysis was performed using equivalent widths and spectral synthesis.
Results. With the new MOST data set from 2011/12 and the two CoRoT light curves from 2008 and 2011/12, the delta Scuti variability was confirmed and regular groups of frequencies were discovered. The two pulsation frequencies identified in the data from the first MOST observing run in 2006 are confirmed and 23 new delta Scuti-type frequencies were discovered using the CoRoT data. Weighted average frequencies for each group were determined and are related to l = 0 and l = 1 p-modes. Evidence for amplitude modulation of the frequencies in two groups is seen. The effective temperature (T-eff) was derived to be 8600 +/- 200K, log g is 4.1 +/- 0.2, and the projected rotational velocity (upsilon sin i) is 53 +/- 1 km s(-1). Using our T-eff value and the radius of 1.8 +/- 0.5 R-circle dot derived from spectral energy distribution (SED) fitting, we get a luminosity log L/L-circle dot of 1.20 +/- 0.14 which agrees well to the seismologically determined values of 1.65 R-circle dot and, hence, a log L/L-circle dot of 1.13. The radial velocity of 14 +/- 2 km s(-1) we derived for HD261711, confirms the star's membership to NGC 2264.
Conclusions. Our asteroseismic models suggest that HD261711 is a delta Scuti-type star close to the zero-age main sequence (ZAMS) with a mass of 1.8 to 1.9 M-circle dot. With an age of about 10 million years derived from asteroseismology, the star is either a young ZAMS star or a late PMS star just before the onset of hydrogen-core burning. The observed splittings about the l = 0 and 1 parent modes may be an artifact of the Fourier derived spectrum of frequencies with varying amplitudes.
C1 [Zwintz, K.] Katholieke Univ Leuven, Inst Sterrenkunde, B-3001 Louvain, Belgium.
[Zwintz, K.; Themessl, N.; Kuschnig, R.; Weiss, W. W.] Univ Vienna, Inst Astron, A-1180 Vienna, Austria.
[Fossati, L.] Univ Bonn, Argelander Inst Astron, D-53121 Bonn, Germany.
[Guenther, D. B.] St Marys Univ, Dept Phys & Astron, Halifax, NS B3H 3C3, Canada.
[Ryabchikova, T.] Russian Acad Sci, Inst Astron, Moscow 119017, Russia.
[Baglin, A.; Auvergne, M.; Chaintreuil, S.] Observ Paris, LESIA, F-92195 Meudon, France.
[Barnes, T. G.] Univ Texas Austin, McDonald Observ, Austin, TX 79734 USA.
[Matthews, J. M.] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada.
[Bohlender, D.] Natl Res Council Canada, Herzberg Inst Astrophys, Victoria, BC V9E 2E7, Canada.
[Moffat, A. F. J.] Univ Montreal, Dept Phys, Montreal, PQ H3C 3J7, Canada.
[Rowe, J. F.] NASA Ames Res Pk, Moffett Field, CA 94035 USA.
[Rucinski, S. M.] Univ Toronto, Dept Astron & Astrophys, Toronto, ON M5S 3H4, Canada.
[Sasselov, D.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Zwintz, K (reprint author), Katholieke Univ Leuven, Inst Sterrenkunde, Celestijnenlaan 200D, B-3001 Louvain, Belgium.
EM konstanze.zwintz@ster.kuleuven.be
OI Zwintz, Konstanze/0000-0001-9229-8315
FU Research Foundation - Flanders (FWO); Austrian Fonds zur Forderung der
wissenschaftlichen Forschung [P 21830-N16, P22691-N16]; Russian Academy
of Sciences "Non-stationary phenomena in the Universe"; Natural Sciences
and Engineering Research Council (NSERC) of Canada; Austrian Research
Promotion Agency-ALR
FX K.Z. receives a Pegasus Marie Curie Fellowship of the Research
Foundation - Flanders (FWO). This investigation has been supported by
the Austrian Fonds zur Forderung der wissenschaftlichen Forschung
through project P 21830-N16 (PI: M. Breger). T.R. acknowledges partial
financial support from Basic Research Program of the Russian Academy of
Sciences "Non-stationary phenomena in the Universe". D.B.G., J.M.,
A.F.J.M. and S.M.R. acknowledge the funding support of the Natural
Sciences and Engineering Research Council (NSERC) of Canada. R.K. and
W.W.W. are supported by the Austrian Fonds zur Forderung der
wissenschaftlichen Forschung (P22691-N16) and by the Austrian Research
Promotion Agency-ALR. Spectroscopic data were obtained with the 2.7-m
telescope at Mc Donald Observatory, Texas, US and at the Dominion
Astrophysical Observatory, Herzberg Institute of Astrophysics, National
Research Council of Canada.
NR 71
TC 5
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U1 0
U2 2
PU EDP SCIENCES S A
PI LES ULIS CEDEX A
PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A,
FRANCE
SN 0004-6361
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD APR
PY 2013
VL 552
AR A68
DI 10.1051/0004-6361/201220934
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 130JW
UT WOS:000317912000068
ER
PT J
AU Lucas, N
Doty, M
Taubert, L
Wygnanski, I
AF Lucas, Nathaniel
Doty, Michael
Taubert, Lutz
Wygnanski, Israel
TI Reducing the noise emanating from a twin jet nozzle using flexible
filaments
SO EXPERIMENTS IN FLUIDS
LA English
DT Article
AB A twin jet was tested in anechoic facilities at the University of Arizona and NASA Langley Research Center to determine the effectiveness of flexible filaments in jet noise reduction. Results were strongly dependent on filament diameter and material, the most effective of which was found to be Tex 800 Kevlar. In the best configurations, the filaments consistently eliminated screech tones and reduced overall sound pressure level by 3 dB or more. Additionally, broadband shock noise was diminished by more than 5 dB over certain audible frequency ranges. Larger-scale tests run at NASA showed comparable reductions in overall sound pressure level and broadband shock-associated noise.
C1 [Lucas, Nathaniel; Taubert, Lutz; Wygnanski, Israel] Univ Arizona, Dept Aerosp & Mech Engn, Tucson, AZ 85721 USA.
[Doty, Michael; Wygnanski, Israel] NASA, Aeroacoust Branch, Langley Res Ctr, Hampton, VA 23681 USA.
RP Lucas, N (reprint author), Univ Arizona, Dept Aerosp & Mech Engn, 1130 N Mt Ave, Tucson, AZ 85721 USA.
EM nlucas333@gmail.com
FU NASA Langley Research Directorate Office; Fundamental Aeronautics
Program Supersonics Project
FX We would like to acknowledge the assistance of Dr. Jesse Little, who was
very helpful in making sure the results and background information were
framed in the proper context with respect to other aeroacoustics
research that has been done in the past, and Philipp Tewes, who
contributed to the data processing effort. Many thanks to Harry Haskin,
John Swartzbaugh, and the rest of the NASA JNL crew for the exciting
opportunity to collaborate our research. Funding for the NASA tests from
the NASA Langley Research Directorate Office and the Fundamental
Aeronautics Program Supersonics Project is gratefully acknowledged.
NR 17
TC 0
Z9 0
U1 2
U2 9
PU SPRINGER
PI NEW YORK
PA 233 SPRING ST, NEW YORK, NY 10013 USA
SN 0723-4864
J9 EXP FLUIDS
JI Exp. Fluids
PD APR
PY 2013
VL 54
IS 4
AR 1504
DI 10.1007/s00348-013-1504-8
PG 10
WC Engineering, Mechanical; Mechanics
SC Engineering; Mechanics
GA 133RX
UT WOS:000318158500014
ER
PT J
AU Saxena, R
Fingland, N
Patil, D
Sharma, AK
Crooke, E
AF Saxena, Rahul
Fingland, Nicholas
Patil, Digvijay
Sharma, Anjali K.
Crooke, Elliott
TI Crosstalk between DnaA Protein, the Initiator of Escherichia coli
Chromosomal Replication, and Acidic Phospholipids Present in Bacterial
Membranes
SO INTERNATIONAL JOURNAL OF MOLECULAR SCIENCES
LA English
DT Review
DE acidic phospholipids; DnaA protein; chromosomal replication; Escherichia
coli
ID OSMOSENSORY TRANSPORTER PROP; DIVISION-SITE SELECTION; UNSATURATED
FATTY-ACIDS; AAA PLUS PROTEIN; CARDIOLIPIN SYNTHESIS; FUNCTIONAL
INTERACTION; AMINO-ACIDS; CELL-CYCLE; IN-VITRO; REGULATORY INACTIVATION
AB Anionic (i.e., acidic) phospholipids such as phosphotidylglycerol (PG) and cardiolipin (CL), participate in several cellular functions. Here we review intriguing in vitro and in vivo evidence that suggest emergent roles for acidic phospholipids in regulating DnaA protein-mediated initiation of Escherichia coli chromosomal replication. In vitro acidic phospholipids in a fluid bilayer promote the conversion of inactive ADP-DnaA to replicatively proficient ATP-DnaA, yet both PG and CL also can inhibit the DNA-binding activity of DnaA protein. We discuss how cellular acidic phospholipids may positively and negatively influence the initiation activity of DnaA protein to help assure chromosomal replication occurs once, but only once, per cell-cycle. Fluorescence microscopy has revealed that PG and CL exist in domains located at the cell poles and mid-cell, and several studies link membrane curvature with sub-cellular localization of various integral and peripheral membrane proteins. E. coli DnaA itself is found at the cell membrane and forms helical structures along the longitudinal axis of the cell. We propose that there is cross-talk between acidic phospholipids in the bacterial membrane and DnaA protein as a means to help control the spatial and temporal regulation of chromosomal replication in bacteria.
C1 [Saxena, Rahul; Patil, Digvijay; Sharma, Anjali K.; Crooke, Elliott] Georgetown Univ, Med Ctr, Dept Biochem & Mol & Cellular Biol, Washington, DC 20007 USA.
[Fingland, Nicholas] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Crooke, Elliott] Georgetown Univ, Med Ctr, Lombardi Comprehens Canc Ctr, Washington, DC 20007 USA.
RP Saxena, R (reprint author), Georgetown Univ, Med Ctr, Dept Biochem & Mol & Cellular Biol, Washington, DC 20007 USA.
EM rs426@georgetown.edu; nick.k.fingland@jpl.nasa.gov;
dap89@georgetown.edu; anjali0623@gmail.com; crooke@georgetown.edu
FU Georgetown University Medical Center Office
FX This work was supported in part by the Georgetown University Medical
Center Office for the Dean for Research.
NR 125
TC 14
Z9 14
U1 2
U2 25
PU MDPI AG
PI BASEL
PA POSTFACH, CH-4005 BASEL, SWITZERLAND
SN 1422-0067
J9 INT J MOL SCI
JI Int. J. Mol. Sci.
PD APR
PY 2013
VL 14
IS 4
BP 8517
EP 8537
DI 10.3390/ijms14048517
PG 21
WC Biochemistry & Molecular Biology; Chemistry, Multidisciplinary
SC Biochemistry & Molecular Biology; Chemistry
GA 131SU
UT WOS:000318017100108
PM 23595001
ER
PT J
AU Korolev, A
Emery, E
Creelman, K
AF Korolev, Alexei
Emery, Edward
Creelman, Kirk
TI Modification and Tests of Particle Probe Tips to Mitigate Effects of Ice
Shattering
SO JOURNAL OF ATMOSPHERIC AND OCEANIC TECHNOLOGY
LA English
DT Article
ID OPTICAL ARRAY PROBES; CRYSTALS; BREAKUP; FSSP; SIZE
AB Ice particle shattering may significantly contaminate measurements taken by airborne particle probes in ice clouds. Environment Canada and the NASA Glenn Research Center (GRC) undertook efforts to modify and test probe tips in order to mitigate the effect of shattering on measurements. This work presents an overview of the results obtained during the design work on the particle probe arm tips. Even though this work was focused on the modifications of three of the probes-Particle Measuring Systems Inc. (PMS) Forward Scattering Spectrometer Probe and optical array probe, and Droplet Measurement Technologies (DMT) Cloud Imaging Probe-the outcomes of this work bear a general character and are applicable to other similar instruments. The results of the airflow analysis around the probe's housing and the simulations of particle bouncing from the probe tips are discussed here. The originally designed and modified tips were tested in a high-speed wind tunnel in ice and liquid sprays. The ice particle bouncing processes as well as patterns of water shedding over the surface of the probes arms were studied with the help of a high-speed video camera. It was found that at aircraft speed, after bouncing from a solid surface, ice particles may travel several centimeters across the airflow and bounce forward up to 1 cm. For the first time it has been directly documented with high-speed video recording that the sample volumes of particle probes with the originally designed tips are contaminated by shattered and bounced particles. A set of recommendations on the existing modification and the design of future particle probe housings is presented.
C1 [Korolev, Alexei] Environm Canada, Cloud Phys & Severe Weather Res Sect, Toronto, ON M3H 5T4, Canada.
[Emery, Edward] NASA Glenn Res Ctr, Cleveland, OH USA.
[Creelman, Kirk] Auriga Design Inc, Haliburton, ON, Canada.
RP Korolev, A (reprint author), Environm Canada, 4905 Dufferin St, Toronto, ON M3H 5T4, Canada.
EM alexei.korolev@ec.gc.ca
FU Environment Canada; Federal Aviation Administration; NASA; Transport
Canada
FX This work was funded by Environment Canada, Transport Canada, the
Federal Aviation Administration, and NASA. The authors express their
gratitude to Cox and Company personnel and, in particular, to Adam
Lawrence for such a high level of cooperation and support in operating
the Cox and Company wind tunnel facility. The NASA Glenn Research Center
video group Vince Reich, Chris Lynch, and Quentin Schwinn did an
excellent job capturing highspeed videos during the Cox and Company wind
tunnel tests. It is hard to overestimate the role of Vladimir Torgashev,
who did mechanical drawing and supervised manufacturing of the probe
tips. Special thanks to Alex Shahshkov of Environment Canada for his
help in data analysis. The authors thank Alain Protat and two anonymous
reviewers for their thoughtful comments.
NR 20
TC 31
Z9 31
U1 2
U2 9
PU AMER METEOROLOGICAL SOC
PI BOSTON
PA 45 BEACON ST, BOSTON, MA 02108-3693 USA
SN 0739-0572
J9 J ATMOS OCEAN TECH
JI J. Atmos. Ocean. Technol.
PD APR
PY 2013
VL 30
IS 4
BP 690
EP 708
DI 10.1175/JTECH-D-12-00142.1
PG 19
WC Engineering, Ocean; Meteorology & Atmospheric Sciences
SC Engineering; Meteorology & Atmospheric Sciences
GA 130YF
UT WOS:000317955700004
ER
PT J
AU Chepfer, H
Cesana, G
Winker, D
Getzewich, B
Vaughan, M
Liu, Z
AF Chepfer, H.
Cesana, G.
Winker, D.
Getzewich, B.
Vaughan, M.
Liu, Z.
TI Comparison of Two Different Cloud Climatologies Derived from
CALIOP-Attenuated Backscattered Measurements (Level 1): The CALIPSO-ST
and the CALIPSO-GOCCP
SO JOURNAL OF ATMOSPHERIC AND OCEANIC TECHNOLOGY
LA English
DT Article
ID TROPICAL TROPOPAUSE; LIDAR; ISCCP; PERFORMANCE; VALIDATION; AEROSOLS;
MISSION; CIRRUS; ECMWF; TERRA
AB Two different cloud climatologies have been derived from the same NASA-Cloud-Aerosol Lidar with Orthogonal Polarization (CALIOP)-measured attenuated backscattered profile (level 1, version 3 dataset). The first climatology, named Cloud-Aerosol Lidar and Infrared Pathfinder Satellite Observations-Science Team (CALIPSO-ST), is based on the standard CALIOP cloud mask (level 2 product, version 3), with the aim to document clouds with the highest possible spatiotemporal resolution, taking full advantage of the CALIOP capabilities and sensitivity for a wide range of cloud scientific studies. The second climatology, named GCM-Oriented CALIPSO Cloud Product (CALIPSO-GOCCP), is aimed at a single goal: evaluating GCM prediction of cloudiness. For this specific purpose, it has been designed to be fully consistent with the CALIPSO simulator included in the Cloud Feedback Model Intercomparison Project (CFMIP) Observation Simulator Package (COSP) used within version 2 of the CFMIP (CFMIP-2) experiment and phase 5 of the Coupled Model Intercomparison Project (CMIP5).
The differences between the two datasets in the global cloud cover maps-total, low level (P > 680 hPa), midlevel (680 < P < 440 hPa), and high level (P < 440 hPa)-are frequently larger than 10% and vary with region.
The two climatologies show significant differences in the zonal cloud fraction profile (which differ by a factor of almost 2 in some regions), which are due to the differences in the horizontal and vertical averaging of the measured attenuated backscattered profile CALIOP profile before the cloud detection and to the threshold used to detect clouds (this threshold depends on the resolution and the signal-to-noise ratio).
C1 [Chepfer, H.] Univ Paris 06, LMD, IPSL, Paris, France.
[Cesana, G.] Ecole Polytech, LMD, IPSL, Palaiseau, France.
[Winker, D.; Vaughan, M.] NASA, Langley Res Ctr, Hampton, VA 23665 USA.
[Getzewich, B.; Liu, Z.] SSAI, Hampton, VA USA.
RP Chepfer, H (reprint author), UPMC, Ecole Polytech, LMD, IPSL, F-91128 Palaiseau, France.
EM helene.chepfer@lmd.polytechnique.fr
RI Liu, Zhaoyan/B-1783-2010
OI Liu, Zhaoyan/0000-0003-4996-5738
NR 40
TC 15
Z9 15
U1 1
U2 22
PU AMER METEOROLOGICAL SOC
PI BOSTON
PA 45 BEACON ST, BOSTON, MA 02108-3693 USA
SN 0739-0572
EI 1520-0426
J9 J ATMOS OCEAN TECH
JI J. Atmos. Ocean. Technol.
PD APR
PY 2013
VL 30
IS 4
BP 725
EP 744
DI 10.1175/JTECH-D-12-00057.1
PG 20
WC Engineering, Ocean; Meteorology & Atmospheric Sciences
SC Engineering; Meteorology & Atmospheric Sciences
GA 130YF
UT WOS:000317955700006
ER
PT J
AU Koskulics, J
Englehardt, S
Long, S
Hu, YX
Ottaviani, M
Stamnes, K
AF Koskulics, Jeffrey
Englehardt, Steven
Long, Steven
Hu, Yongxiang
Ottaviani, Matteo
Stamnes, Knut
TI Water Surface Topography Retrieved from Color Images
SO JOURNAL OF ATMOSPHERIC AND OCEANIC TECHNOLOGY
LA English
DT Article
ID ATMOSPHERE-OCEAN SYSTEM; WIND-WAVES; MULTIANGLE; RADIANCES; SLOPES
AB Submerged objects viewed through wavy water surfaces appear distorted by refraction. An imaging system exploiting this effect is implemented using a submerged planar light source designed so that color images reveal features of small-amplitude waves in a wind-wave tank. The system is described by a nonlinear model of image formation based on the geometry of refraction, spectral emission from the light source, radiative transfer through the water and surface, and camera spectral response. Surface normal vector components are retrieved from the color image data using an iterative solution to the nonlinear model. The surface topography is then retrieved using a linear model that combines surface normal data with a priori constraints on elevation and curvature. The high-resolution topographic data reveal small-amplitude waves spanning wavelength scales from capillary through short gravity wave regimes. The system capabilities are demonstrated in the retrieval of test surfaces, and of a case of wind-driven waves, using data collected at high spatial and temporal resolution in a wave tank. The approach of using a physical model of image formation with inverse solution methods provides an example of how surface topography can be retrieved and may be applicable to data from other similar instruments.
C1 [Koskulics, Jeffrey; Englehardt, Steven; Stamnes, Knut] Stevens Inst Technol, Hoboken, NJ 07030 USA.
[Long, Steven] NASA, Goddard Space Flight Ctr, Air Sea Interact Res Facil, Wallops Flight Facil, Wallops Isl, VA 23337 USA.
[Hu, Yongxiang] NASA, Langley Res Ctr, Hampton, VA 23665 USA.
[Ottaviani, Matteo] NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
RP Koskulics, J (reprint author), Stevens Inst Technol, Light & Life Lab, 1 Castle Point Hudson, Hoboken, NJ 07030 USA.
EM jkoskuli@stevens.edu
RI Hu, Yongxiang/K-4426-2012
FU NASA Radiation Sciences Program
FX The authors acknowledge support from the NASA Radiation Sciences Program
and wish to thank the program manager, Dr. Hal Maring. SRL would like to
express his thanks to Dr. Eric Lindstrom of the NASA Science Mission
Directorate for supporting the research efforts of NASIRF during its
final years of operation.
NR 29
TC 0
Z9 0
U1 0
U2 6
PU AMER METEOROLOGICAL SOC
PI BOSTON
PA 45 BEACON ST, BOSTON, MA 02108-3693 USA
SN 0739-0572
EI 1520-0426
J9 J ATMOS OCEAN TECH
JI J. Atmos. Ocean. Technol.
PD APR
PY 2013
VL 30
IS 4
BP 846
EP 860
DI 10.1175/JTECH-D-12-00047.1
PG 15
WC Engineering, Ocean; Meteorology & Atmospheric Sciences
SC Engineering; Meteorology & Atmospheric Sciences
GA 130YF
UT WOS:000317955700012
ER
PT J
AU Reynolds, RW
Chelton, DB
Roberts-Jones, J
Martin, MJ
Menemenlis, D
Merchant, CJ
AF Reynolds, Richard W.
Chelton, Dudley B.
Roberts-Jones, Jonah
Martin, Matthew J.
Menemenlis, Dimitris
Merchant, Christopher John
TI Objective Determination of Feature Resolution in Two Sea Surface
Temperature Analyses
SO JOURNAL OF CLIMATE
LA English
DT Article
ID OCEAN; MODEL; CLIMATE
AB Considerable effort is presently being devoted to producing high-resolution sea surface temperature (SST) analyses with a goal of spatial grid resolutions as low as 1 km. Because grid resolution is not the same as feature resolution, a method is needed to objectively determine the resolution capability and accuracy of SST analysis products. Ocean model SST fields are used in this study as simulated "true'' SST data and subsampled based on actual infrared and microwave satellite data coverage. The subsampled data are used to simulate sampling errors due to missing data. Two different SST analyses are considered and run using both the full and the subsampled model SST fields, with and without additional noise. The results are compared as a function of spatial scales of variability using wavenumber auto-and cross-spectral analysis.
The spectral variance at high wavenumbers (smallest wavelengths) is shown to be attenuated relative to the true SST because of smoothing that is inherent to both analysis procedures. Comparisons of the two analyses (both having grid sizes of roughly 1/20 degrees) show important differences. One analysis tends to reproduce small-scale features more accurately when the high-resolution data coverage is good but produces more spurious small-scale noise when the high-resolution data coverage is poor. Analysis procedures can thus generate small-scale features with and without data, but the small-scale features in an SST analysis may be just noise when high-resolution data are sparse. Users must therefore be skeptical of high-resolution SST products, especially in regions where high-resolution ( similar to 5 km) infrared satellite data are limited because of cloud cover.
C1 [Reynolds, Richard W.] N Carolina State Univ, Cooperat Inst Climate & Satellites, Asheville, NC USA.
[Reynolds, Richard W.] NOAA, Natl Climat Data Ctr, Asheville, NC 28801 USA.
[Chelton, Dudley B.] Oregon State Univ, Coll Ocean & Atmospher Sci, Corvallis, OR 97331 USA.
[Chelton, Dudley B.] Oregon State Univ, Cooperat Inst Oceanog Satellite Studies, Corvallis, OR 97331 USA.
[Roberts-Jones, Jonah; Martin, Matthew J.] Met Off, Exeter, Devon, England.
[Menemenlis, Dimitris] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Merchant, Christopher John] Univ Edinburgh, Edinburgh, Midlothian, Scotland.
RP Reynolds, RW (reprint author), NOAA, Cooperat Inst Climate & Satellites, 151 Patton Ave, Asheville, NC 28801 USA.
EM richard.w.reynolds@noaa.gov
RI Merchant, Christopher/E-1180-2014
OI Merchant, Christopher/0000-0003-4687-9850
FU NOAA's Climate Data Record Program; NCDC; NOAA/Climate Program Office;
NASA Grant through Oregon State University [NS214A]; European Community
[283367]; NASA
FX This work was funded in part by NOAA's Climate Data Record Program,
managed by the National Climatic Data Center. We are grateful to NCDC
and the NOAA/Climate Program Office, which provided partial support for
this work. The graphics for all of the figures were computed using the
Grid Analysis and Display System (GrADS; available online at
http://grads.iges.org/grads) and finalized by the NCDC Graphics
Department. Both DCB and RWR were partially supported by NASA Grant
NS214A funded through Oregon State University. The research of JRJ and
MJM leading to these results has received funding from the European
Community's Seventh Framework Programme FP7/2007-2013 under Grant
Agreement 283367 (MyOcean 2). DM performed this work at the Jet
Propulsion Laboratory, California Institute of Technology, under
contract with NASA.
NR 19
TC 4
Z9 4
U1 1
U2 14
PU AMER METEOROLOGICAL SOC
PI BOSTON
PA 45 BEACON ST, BOSTON, MA 02108-3693 USA
SN 0894-8755
J9 J CLIMATE
JI J. Clim.
PD APR
PY 2013
VL 26
IS 8
BP 2514
EP 2533
DI 10.1175/JCLI-D-12-00787.1
PG 20
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 130XX
UT WOS:000317954700007
ER
PT J
AU Tatarinova, T
Neely, M
Bartroff, J
van Guilder, M
Yamada, W
Bayard, D
Jelliffe, R
Leary, R
Chubatiuk, A
Schumitzky, A
AF Tatarinova, Tatiana
Neely, Michael
Bartroff, Jay
van Guilder, Michael
Yamada, Walter
Bayard, David
Jelliffe, Roger
Leary, Robert
Chubatiuk, Alyona
Schumitzky, Alan
TI Two general methods for population pharmacokinetic modeling:
non-parametric adaptive grid and non-parametric Bayesian
SO JOURNAL OF PHARMACOKINETICS AND PHARMACODYNAMICS
LA English
DT Article
DE Population pharmacokinetic modeling; Non-parametric; Maximum likelihood;
Bayesian; Stick-breaking; Pmetrics; RJags
ID CHAIN MONTE-CARLO; PARAMETERS; SIMULATION; PRIORS
AB Population pharmacokinetic (PK) modeling methods can be statistically classified as either parametric or nonparametric (NP). Each classification can be divided into maximum likelihood (ML) or Bayesian (B) approaches. In this paper we discuss the nonparametric case using both maximum likelihood and Bayesian approaches. We present two nonparametric methods for estimating the unknown joint population distribution of model parameter values in a pharmacokinetic/pharmacodynamic (PK/PD) dataset. The first method is the NP Adaptive Grid (NPAG). The second is the NP Bayesian (NPB) algorithm with a stick-breaking process to construct a Dirichlet prior. Our objective is to compare the performance of these two methods using a simulated PK/PD dataset. Our results showed excellent performance of NPAG and NPB in a realistically simulated PK study. This simulation allowed us to have benchmarks in the form of the true population parameters to compare with the estimates produced by the two methods, while incorporating challenges like unbalanced sample times and sample numbers as well as the ability to include the covariate of patient weight. We conclude that both NPML and NPB can be used in realistic PK/PD population analysis problems. The advantages of one versus the other are discussed in the paper. NPAG and NPB are implemented in R and freely available for download within the Pmetrics package from www.lapk.org.
C1 [Tatarinova, Tatiana; Neely, Michael; Bartroff, Jay; van Guilder, Michael; Yamada, Walter; Bayard, David; Jelliffe, Roger; Leary, Robert; Schumitzky, Alan] Univ So Calif, Keck Sch Med, Lab Appl Pharmacokinet, Los Angeles, CA 90033 USA.
[Bartroff, Jay; Chubatiuk, Alyona; Schumitzky, Alan] Univ So Calif, Dept Math, Dornsife Coll Letters & Sci, Los Angeles, CA 90089 USA.
[Yamada, Walter] Azusa Pacific Univ, Dept Psychol, Azusa, CA USA.
[Bayard, David] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Leary, Robert] Pharsight Corp, Cary, NC USA.
RP Tatarinova, T (reprint author), Univ So Calif, Keck Sch Med, Lab Appl Pharmacokinet, Los Angeles, CA 90033 USA.
EM tatiana.tatarinova@lapk.org
RI Tatarinova, Tatiana/K-3445-2016
OI Tatarinova, Tatiana/0000-0003-1787-1112
FU NIH [GM068968, EB005803, EB001978]; NIH-NICHD [HD070996]; Royal Society
[TG103083]
FX Support from NIH: GM068968, EB005803, EB001978, NIH-NICHD: HD070996 and
Royal Society: TG103083 is gratefully acknowledged.
NR 43
TC 25
Z9 25
U1 2
U2 8
PU SPRINGER/PLENUM PUBLISHERS
PI NEW YORK
PA 233 SPRING ST, NEW YORK, NY 10013 USA
SN 1567-567X
EI 1573-8744
J9 J PHARMACOKINET PHAR
JI J. Pharmacokinet. Pharmacodyn.
PD APR
PY 2013
VL 40
IS 2
BP 189
EP 199
DI 10.1007/s10928-013-9302-8
PG 11
WC Pharmacology & Pharmacy
SC Pharmacology & Pharmacy
GA 131EC
UT WOS:000317974200005
PM 23404393
ER
PT J
AU Sears, DWG
AF Sears, Derek W. G.
TI Oral Histories in Meteoritics and Planetary Science - XX: Dale
Cruikshank
SO METEORITICS & PLANETARY SCIENCE
LA English
DT Article
ID SATELLITES; TRITON; ATMOSPHERE; ASTEROIDS; SURFACE; PLUTO; ICES; IO
AB In this interview, Dale Cruikshank (Fig.1) explains how as an undergraduate at Iowa State University he was a summer student at Yerkes Observatory where he assisted Gerard Kuiper in work on his Photographic Lunar Atlas. Upon completing his degree, Dale went to graduate school at the University of Arizona with Kuiper where he worked on the IR spectroscopy of the lunar surface. After an eventful 1968 trip to Moscow via Prague, during which the Soviets invaded Czechoslovakia, Dale assumed a postdoc position with Vasili Moroz at the Sternberg Astronomical Institute and more observational IR astronomy. Upon returning to the United States and after a year at Arizona, Dale assumed a position at the University of Hawai'i that he held for 17years. During this period Dale worked with others on thermal infrared determinations of the albedos of small bodies beyond the asteroid Main Belt, leading to the recognition that low-albedo material is prevalent in the outer solar system that made the first report of complex organic solids on a planetary body (Saturn's satellite Iapetus). After moving to Ames Research Center, where he works currently, he continued this work and became involved in many outer solar system missions. Dale has served the community through his involvement in developing national policies for science-driven planetary exploration, being chair of the DPS 19901991 and secretary/treasurer for 19821985. He served as president of Commission 16 (Physics of Planets) of the IAU (20012003). He received the Kuiper prize in 2006. 1 Dale P. Cruikshank.
C1 NASA, Ames Res Ctr, Planetary Sci & Astrobiol Div, Mountain View, CA 94035 USA.
RP Sears, DWG (reprint author), NASA, Ames Res Ctr, Planetary Sci & Astrobiol Div, Mountain View, CA 94035 USA.
EM derek.sears@nasa.gov
FU NASA
FX This interview was recorded on March 16, 2011, and edited by the author
and DPC. I am grateful to Klaus Keil for a review and Hazel Sears for
reviewing and proofing this article. A grant from NASA supported the
work.
NR 16
TC 0
Z9 0
U1 0
U2 1
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 1086-9379
J9 METEORIT PLANET SCI
JI Meteorit. Planet. Sci.
PD APR
PY 2013
VL 48
IS 4
BP 700
EP 711
DI 10.1111/j.1945-5100.2012.01414.x
PG 12
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 131WU
UT WOS:000318029400008
ER
PT J
AU Handler, G
Prinja, RK
Urbaneja, MA
Antoci, V
Twicken, JD
Barclay, T
AF Handler, G.
Prinja, R. K.
Urbaneja, M. A.
Antoci, V.
Twicken, J. D.
Barclay, T.
TI Kepler photometry and optical spectroscopy of the ZZ Lep central star of
the planetary nebula NGC 6826: rotational and wind variability
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE stars: early-type; stars: mass-loss; stars: rotation; stars: winds,
outflows; planetary nebulae: individual: NGC 6826
ID COROTATING INTERACTION REGIONS; O-TYPE STARS; INITIAL CHARACTERISTICS;
CADENCE DATA; ASTEROSEISMOLOGY; ULTRAVIOLET; EVOLUTION; SCIENCE
AB We present three years of long-cadence and over one year of short-cadence photometry of the central star of the planetary nebula NGC 6826 obtained with the Kepler spacecraft, and temporally coinciding optical spectroscopy. The light curves are dominated by incoherent variability on time-scales of several hours, but contain a lower amplitude periodicity of 1.237 99 d. The temporal amplitude and shape changes of this signal are best explicable with a rotational modulation, and are not consistent with a binary interpretation. We argue that we do not observe stellar pulsations within the limitations of our data, and show that a binary central star with an orbital period less than seven days could only have escaped our detection in the case of low orbital inclination. Combining the photometric and spectroscopic evidence, we reason that the hourly variations are due to a variable stellar wind, and are global in nature. The physical cause of the wind variability of NGC 6826 and other ZZ Leporis stars is likely related to the mechanism responsible for wind variations in massive hot stars.
C1 [Handler, G.] Copernicus Astron Ctr, PL-00716 Warsaw, Poland.
[Prinja, R. K.] UCL, Dept Phys & Astron, London WC1E 6BT, England.
[Urbaneja, M. A.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA.
[Antoci, V.] Aarhus Univ, Dept Phys & Astron, SAC, DK-8000 Aarhus C, Denmark.
[Antoci, V.] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada.
[Twicken, J. D.] NASA, Ames Res Ctr, SETI Inst, Moffett Field, CA 94035 USA.
[Barclay, T.] NASA, Ames Res Ctr, Bay Area Environm Res Inst, Moffett Field, CA 94035 USA.
RP Handler, G (reprint author), Copernicus Astron Ctr, Bartycka 18, PL-00716 Warsaw, Poland.
EM gerald@camk.edu.pl
OI Antoci, Victoria/0000-0002-0865-3650
FU NASA's Science Mission Directorate; Danish National Research Foundation;
ASTERISK project; European Research Council [267864]; NCN
[2011/01/B/ST9/05448]
FX Funding for this Discovery mission is provided by NASA's Science Mission
Directorate. The authors thank the Kepler team for their continuous work
that ensures the best possible science output. Funding for the Stellar
Astrophysics Centre (SAC) is provided by The Danish National Research
Foundation. The research is supported by the ASTERISK project
(ASTERoseismic Investigations with SONG and Kepler) funded by the
European Research Council (Grant agreement no.: 267864). The authors
would like to thank S. Simon-Diaz for his assistance with the FIES/NOT
observations. GH acknowledges funding through NCN grant
2011/01/B/ST9/05448, and thanks Nada Jevtic and Andrzej Baran for their
comments on a draft version of this paper. Comments by the anonymous
referee improved part of our argumentation. This paper is partly based
on observations made with the Nordic Optical Telescope operated on the
island of La Palma by the Nordic Optical Telescope Scientific
Association in the Spanish Observatorio del Roque de los Muchachos.
NR 41
TC 5
Z9 5
U1 0
U2 4
PU OXFORD UNIV PRESS
PI OXFORD
PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND
SN 0035-8711
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD APR
PY 2013
VL 430
IS 4
BP 2923
EP 2931
DI 10.1093/mnras/stt092
PG 9
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 136CZ
UT WOS:000318339700035
ER
PT J
AU Zhou, Y
Isheim, D
Hsieh, G
Noebe, RD
Seidman, DN
AF Zhou, Yang
Isheim, Dieter
Hsieh, Gillian
Noebe, Ronald D.
Seidman, David N.
TI Effects of ruthenium on phase separation in a model NiAlCrRu superalloy
SO PHILOSOPHICAL MAGAZINE
LA English
DT Article
DE NiAlCrRu alloy; effects of Ru; coarseniing kinetics; atom-probe
tomography; transmission electron microscopy
ID NICKEL-BASE SUPERALLOYS; SINGLE-CRYSTAL SUPERALLOYS; NI-CR-AL;
3-DIMENSIONAL ATOM-PROBE; OSTWALD RIPENING THEORIES;
MONTE-CARLO-SIMULATION; TEMPORAL EVOLUTION; GAMMA'-PHASE; MULTICOMPONENT
ALLOYS; KINETIC PATHWAYS
AB The temporal evolution of a Ni10.0Al8.5Cr2.0Ru (at.%) alloy aged at 1073K was investigated using transmission electron microscopy (TEM) and atom-probe tomography. The (L1(2))-precipitate morphology is spheroidal through 256h of ageing as a result of adding Ru, which decreases the lattice parameter misfit between the (L1(2))- and (f.c.c.)-phases. The addition of Ru accelerates the compositional evolution of the (L1(2))- and (f.c.c.)-phases, which achieve their equilibrium compositions after 0.25h. Initially, Ru accelerates the partitioning of Ni and Cr to the (f.c.c.)-phase, and the partitioning of Al to the (L1(2))-phase, but after 0.25h, Ru, which partitions to the (f.c.c.)-phase, decreases the partitioning of Ni and increases the partitioning of Al and Cr. The temporal evolution of the average radius, R(t), number density, volume fraction of the (L1(2))-precipitates, and the supersaturations of Ni, Al, Cr, and Ru in the (f.c.c.)- and (L1(2))-phases are compared in detail with predictions of coarsening models and PrecipiCalc simulations. Based on a spline function fitting procedure of the concentration profiles between the (L1(2))- and (f.c.c.)-phases, it is demonstrated that the temporal evolution of the normalized interfacial width, /R(t) vs.R(t), of each element, decreases with increasing ageing time: is the interfacial width.
C1 [Zhou, Yang; Isheim, Dieter; Hsieh, Gillian; Seidman, David N.] Northwestern Univ, Dept Mat Sci & Engn, Evanston, IL 60208 USA.
[Zhou, Yang] Micron Technol Inc, Surface Anal Lab, Boise, ID 83707 USA.
[Noebe, Ronald D.] NASA, Glenn Res Ctr, Struct & Mat Div, Cleveland, OH 44135 USA.
[Isheim, Dieter; Seidman, David N.] Northwestern Univ, Ctr Atom Probe Tomog NUCAPT, Mat Res Sci & Engn Ctr, Evanston, IL 60208 USA.
RP Seidman, DN (reprint author), Northwestern Univ, Dept Mat Sci & Engn, 2220 Campus Dr, Evanston, IL 60208 USA.
EM d-seidman@northwestern.edu
RI Seidman, David/B-6697-2009
FU National Science Foundation (NSF) [DMR-0804610]; NSF-NSEC; NSF-MRSEC;
Keck Foundation; State of Illinois; Northwestern University; NSF-MRI
[DMR-0420, 532]; ONR-DURIP [N00014-0400, 798, N00014-0610539,
NOOO14-0910, 781]
FX This research was sponsored by the National Science Foundation (NSF)
under grant DMR-0804610. The TEM studies were performed in the EPIC
facility of the NUANCE Center at Northwestern University. The NUANCE
Center is supported by NSF-NSEC, NSF-MRSEC, the Keck Foundation, the
State of Illinois and Northwestern University. Atom-probe tomographic
measurements were performed in the Northwestern University Center for
Atom-Probe Tomography (NUCAPT). The LEAP tomograph was purchased and
upgraded with funding from NSF-MRI (DMR-0420,532) and ONR-DURIP
(N00014-0400,798, N00014-0610539, NOOO14-0910,781) grants. Ms. Gillian
Hsieh's contributions to this article constitute portions of her senior
thesis in the Department of Material Science and Engineering: she was
also supported by a NSF REU during one summer. Dr Jou at Questek
Inovations LLC is kindly thanked for help with PrecipiCalc simulations,
Dr Chantal K. Sudbrack is thanked for performing the JMat Pro
calculations and reading the manuscript, Drs Christopher Booth-Morrison
and Yaron Amouyal are thanked for helpful discussions and Dr Carelyn
Campbell (NIST) for diffusivity databases.
NR 113
TC 3
Z9 3
U1 0
U2 20
PU TAYLOR & FRANCIS LTD
PI ABINGDON
PA 4 PARK SQUARE, MILTON PARK, ABINGDON OX14 4RN, OXON, ENGLAND
SN 1478-6435
J9 PHILOS MAG
JI Philos. Mag.
PD APR 1
PY 2013
VL 93
IS 10-12
SI SI
BP 1326
EP 1350
DI 10.1080/14786435.2013.765989
PG 25
WC Materials Science, Multidisciplinary; Metallurgy & Metallurgical
Engineering; Physics, Applied; Physics, Condensed Matter
SC Materials Science; Metallurgy & Metallurgical Engineering; Physics
GA 129LO
UT WOS:000317841300014
ER
PT J
AU Aunai, N
Hesse, M
Black, C
Evans, R
Kuznetsova, M
AF Aunai, Nicolas
Hesse, Michael
Black, Carrie
Evans, Rebekah
Kuznetsova, Maria
TI Influence of the dissipation mechanism on collisionless magnetic
reconnection in symmetric and asymmetric current layers
SO PHYSICS OF PLASMAS
LA English
DT Article
ID MAGNETOPAUSE; SIMULATIONS; CHALLENGE; REGION; SHEET
AB Numerical studies implementing different versions of the collisionless Ohm's law have shown a reconnection rate insensitive to the nature of the non-ideal mechanism occurring at the X line, as soon as the Hall effect is operating. Consequently, the dissipation mechanism occurring in the vicinity of the reconnection site in collisionless systems is usually thought not to have a dynamical role beyond the violation of the frozen-in condition. The interpretation of recent studies has, however, led to the opposite conclusion that the electron scale dissipative processes play an important dynamical role in preventing an elongation of the electron layer from throttling the reconnection rate. This work re-visits this topic with a new approach. Instead of focusing on the extensively studied symmetric configuration, we aim to investigate whether the macroscopic properties of collisionless reconnection are affected by the dissipation physics in asymmetric configurations, for which the effect of the Hall physics is substantially modified. Because it includes all the physical scales a priori important for collisionless reconnection (Hall and ion kinetic physics) and also because it allows one to change the nature of the non-ideal electron scale physics, we use a (two dimensional) hybrid model. The effects of numerical, resistive, and hyper-resistive dissipation are studied. In a first part, we perform simulations of symmetric reconnection with different non-ideal electron physics. We show that the model captures the already known properties of collisionless reconnection. In a second part, we focus on an asymmetric configuration where the magnetic field strength and the density are both asymmetric. Our results show that contrary to symmetric reconnection, the asymmetric model evolution strongly depends on the nature of the mechanism which breaks the field line connectivity. The dissipation occurring at the X line plays an important role in preventing the electron current layer from elongating and forming plasmoids. (C) 2013 American Institute of Physics. [http://dx.doi.org/10.1063/1.4795727]
C1 [Aunai, Nicolas; Hesse, Michael; Black, Carrie; Evans, Rebekah; Kuznetsova, Maria] NASA, Space Weather Lab, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Aunai, N (reprint author), NASA, Space Weather Lab, Goddard Space Flight Ctr, Code 674, Greenbelt, MD 20771 USA.
EM nicolas.aunai@nasa.gov
RI feggans, john/F-5370-2012; NASA MMS, Science Team/J-5393-2013
OI NASA MMS, Science Team/0000-0002-9504-5214
FU NASA
FX Three of us (N.A., C. B., and R. E.) acknowledge support from the NASA
postdoctoral program. The authors acknowledge Roch Smets for the hybrid
code.
NR 41
TC 7
Z9 7
U1 1
U2 6
PU AMER INST PHYSICS
PI MELVILLE
PA CIRCULATION & FULFILLMENT DIV, 2 HUNTINGTON QUADRANGLE, STE 1 N O 1,
MELVILLE, NY 11747-4501 USA
SN 1070-664X
J9 PHYS PLASMAS
JI Phys. Plasmas
PD APR
PY 2013
VL 20
IS 4
AR 042901
DI 10.1063/1.4795727
PG 13
WC Physics, Fluids & Plasmas
SC Physics
GA 134UY
UT WOS:000318241900051
ER
PT J
AU Denneau, L
Jedicke, R
Grav, T
Granvik, M
Kubica, J
Milani, A
Veres, P
Wainscoat, R
Chang, D
Pierfederici, F
Kaiser, N
Chambers, KC
Heasley, JN
Magnier, EA
Price, PA
Myers, J
Kleyna, J
Hsieh, H
Farnocchia, D
Waters, C
Sweeney, WH
Green, D
Bolin, B
Burgett, WS
Morgan, JS
Tonry, JL
Hodapp, KW
Chastel, S
Chesley, S
Fitzsimmons, A
Holman, M
Spahr, T
Tholen, D
Williams, GV
Abe, S
Armstrong, JD
Bressi, TH
Holmes, R
Lister, T
McMillan, RS
Micheli, M
Ryan, EV
Ryan, WH
Scotti, JV
AF Denneau, Larry
Jedicke, Robert
Grav, Tommy
Granvik, Mikael
Kubica, Jeremy
Milani, Andrea
Veres, Peter
Wainscoat, Richard
Chang, Daniel
Pierfederici, Francesco
Kaiser, N.
Chambers, K. C.
Heasley, J. N.
Magnier, Eugene A.
Price, P. A.
Myers, Jonathan
Kleyna, Jan
Hsieh, Henry
Farnocchia, Davide
Waters, Chris
Sweeney, W. H.
Green, Denver
Bolin, Bryce
Burgett, W. S.
Morgan, J. S.
Tonry, John L.
Hodapp, K. W.
Chastel, Serge
Chesley, Steve
Fitzsimmons, Alan
Holman, Matthew
Spahr, Tim
Tholen, David
Williams, Gareth V.
Abe, Shinsuke
Armstrong, J. D.
Bressi, Terry H.
Holmes, Robert
Lister, Tim
McMillan, Robert S.
Micheli, Marco
Ryan, Eileen V.
Ryan, William H.
Scotti, James V.
TI The Pan-STARRS Moving Object Processing System
SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF THE PACIFIC
LA English
DT Article
ID EARTH-APPROACHING ASTEROIDS; SYNOPTIC SURVEY TELESCOPE; ORBIT
DETERMINATION; SIZE DISTRIBUTION; POPULATION; SPACEWATCH;
IDENTIFICATION; CALIBRATION; PROGRAM; ARRAY
AB We describe the Pan-STARRS Moving Object Processing System (MOPS), a modern software package that produces automatic asteroid discoveries and identifications from catalogs of transient detections from next-generation astronomical survey telescopes. MOPS achieves >99.5% efficiency in producing orbits from a synthetic but realistic population of asteroids whose measurements were simulated for a Pan-STARRS4-class telescope. Additionally, using a nonphysical grid population, we demonstrate that MOPS can detect populations of currently unknown objects such as interstellar asteroids. MOPS has been adapted successfully to the prototype Pan-STARRS1 telescope despite differences in expected false detection rates, fill-factor loss, and relatively sparse observing cadence compared to a hypothetical Pan-STARRS4 telescope and survey. MOPS remains highly efficient at detecting objects but drops to 80% efficiency at producing orbits. This loss is primarily due to configurable MOPS processing limits that are not yet tuned for the Pan-STARRS1 mission. The core MOPS software package is the product of more than 15 person-years of software development and incorporates countless additional years of effort in third-party software to perform lower-level functions such as spatial searching or orbit determination. We describe the high-level design of MOPS and essential subcomponents, the suitability of MOPS for other survey programs, and suggest a road map for future MOPS development.
C1 [Denneau, Larry; Jedicke, Robert; Veres, Peter; Wainscoat, Richard; Chang, Daniel; Kaiser, N.; Chambers, K. C.; Heasley, J. N.; Magnier, Eugene A.; Kleyna, Jan; Hsieh, Henry; Waters, Chris; Sweeney, W. H.; Green, Denver; Bolin, Bryce; Burgett, W. S.; Morgan, J. S.; Tonry, John L.; Hodapp, K. W.; Chastel, Serge; Tholen, David; Armstrong, J. D.; Micheli, Marco] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA.
[Grav, Tommy] Johns Hopkins Univ, Baltimore, MD USA.
[Granvik, Mikael] Univ Helsinki, Dept Phys, FIN-00014 Helsinki, Finland.
[Milani, Andrea; Farnocchia, Davide] Univ Pisa, Pisa, Italy.
[Pierfederici, Francesco] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
[Price, P. A.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA.
[Myers, Jonathan] Univ Arizona, Tucson, AZ USA.
[Farnocchia, Davide; Chesley, Steve] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Fitzsimmons, Alan] Queens Univ Belfast, Astrophys Res Ctr, Sch Math & Phys, Belfast BT7 1NN, Antrim, North Ireland.
[Holman, Matthew] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Spahr, Tim; Williams, Gareth V.] Smithsonian Astrophys Observ, Cambridge, MA USA.
[Abe, Shinsuke] Natl Cent Univ, Inst Astron, Taipei, Taiwan.
[Bressi, Terry H.; McMillan, Robert S.; Scotti, James V.] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA.
[Holmes, Robert] Astron Res Inst, Charleston, IL 61920 USA.
[Lister, Tim] Las Cumbres Observ Global Telescope Network Inc, Santa Barbara, CA 93117 USA.
[Ryan, Eileen V.; Ryan, William H.] New Mexico Inst Min & Technol, Magdalena Ridge Observ, Socorro, NM 87801 USA.
RP Denneau, L (reprint author), Univ Hawaii, Inst Astron, 2680 Woodlawn Dr, Honolulu, HI 96822 USA.
EM denneau@ifa.hawaii.edu
OI Chambers, Kenneth /0000-0001-6965-7789; Granvik,
Mikael/0000-0002-5624-1888; Micheli, Marco/0000-0001-7895-8209
FU National Aeronautics and Space Administration issued through the
Planetary Science Division of the NASA Science Mission Directorate
[NNX08AR22G]; United States Air Force Research Laboratory (AFRL,
Albuquerque, NM) [F29601-02-1-0268]; Large Synoptic Survey Telescope
(LSST) Corporation
FX The Pan-STARRS1 Survey has been made possible through contributions of
the Institute for Astronomy, the University of Hawai'i, the Pan-STARRS
Project Office, the Max-Planck Society and its participating institutes,
the Max Planck Institute for Astronomy, Heidelberg and the Max Planck
Institute for Extraterrestrial Physics, Garching, The Johns Hopkins
University, Durham University, the University of Edinburgh, Queen's
University Belfast, the Harvard-Smithsonian Center for Astrophysics, and
the Las Cumbres Observatory Global Telescope Network, Incorporated, the
National Central University of Taiwan, and the National Aeronautics and
Space Administration under Grant No. NNX08AR22G issued through the
Planetary Science Division of the NASA Science Mission Directorate.; The
design and construction of the Panoramic Survey Telescope and Rapid
Response System by the University of Hawaii Institute for Astronomy was
funded by the United States Air Force Research Laboratory (AFRL,
Albuquerque, NM) through grant number F29601-02-1-0268.; We acknowledge
the financial and technical contributions to this work made by the Large
Synoptic Survey Telescope (LSST) Corporation team, in particular Tim
Axelrod, Lynne Jones and Jeff Kantor. In addition, we acknowledge the
support by Pan-STARRS and LSST management to enable and facilitate this
productive collaborative effort between the two projects.
NR 59
TC 30
Z9 30
U1 0
U2 5
PU UNIV CHICAGO PRESS
PI CHICAGO
PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA
SN 0004-6280
J9 PUBL ASTRON SOC PAC
JI Publ. Astron. Soc. Pac.
PD APR
PY 2013
VL 125
IS 926
BP 357
EP 395
DI 10.1086/670337
PG 39
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 131BM
UT WOS:000317965800004
ER
PT J
AU Dixon, WV
Blair, WP
Kruk, JW
Romelfanger, ML
AF Dixon, William V.
Blair, William P.
Kruk, Jeffrey W.
Romelfanger, Mary L.
TI The Hopkins Ultraviolet Telescope: The Final Archive
SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF THE PACIFIC
LA English
DT Article
ID CALIBRATION; MISSION; PERFORMANCE; ASTRONOMY; SPECTRUM
AB The Hopkins Ultraviolet Telescope (HUT) was a 0.9 m telescope and moderate-resolution (Delta lambda = 3 angstrom) far-ultraviolet (820-1850 angstrom) spectrograph that flew twice on the space shuttle, in 1990 December (Astro-1, STS-35) and 1995 March (Astro-2, STS-67). The resulting spectra were originally archived in a nonstandard format that lacked important descriptive metadata. To increase their utility, we have modified the original data-reduction software to produce a new and more user-friendly data product, a time-tagged photon list similar in format to the Intermediate Data Files (IDFs) produced by the Far Ultraviolet Spectroscopic Explorer calibration pipeline. We have transferred all relevant pointing and instrument-status information from locally-archived science and engineering databases into new FITS header keywords for each data set. Using this new pipeline, we have reprocessed the entire HUT archive from both missions, producing a new set of calibrated spectral products in a modern FITS format that is fully compliant with Virtual Observatory requirements. For each exposure, we have generated quick-look plots of the fully-calibrated spectrum and associated pointing history information. Finally, we have retrieved from our archives HUT TV guider images, which provide information on aperture positioning relative to guide stars, and converted them into FITS-format image files. All of these new data products are available in the new HUT section of the Mikulski Archive for Space Telescopes (MAST), along with historical and reference documents from both missions. In this article, we document the improved data-processing steps applied to the data and show examples of the new data products.
C1 [Dixon, William V.] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
[Blair, William P.; Romelfanger, Mary L.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA.
[Kruk, Jeffrey W.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Dixon, WV (reprint author), Space Telescope Sci Inst, 3700 San Martin Dr, Baltimore, MD 21218 USA.
EM dixon@stsci.edu; wpb@pha.jhu.edu; Jeffrey.W.Kruk@nasa.gov;
mary@pha.jhu.edu
FU NASA ADP Grant [NNX09AC70G]; Center for Astrophysical Sciences at the
Johns Hopkins University; NASA [NAS5-26555]; NASA Office of Space
Science [NAG5-7584]
FX This work has been supported by NASA ADP Grant #NNX09AC70G to the Johns
Hopkins University and by the Center for Astrophysical Sciences at the
Johns Hopkins University. It has made use of NASA's Astrophysics Data
System Bibliographic Services (ADS) and the Mikulski Archive for Space
Telescopes (MAST), hosted at the Space Telescope Science Institute.
STScI is operated by the Association of Universities for Research in
Astronomy, Inc., under NASA contract NAS5-26555. Support for MAST for
non-HST data is provided by the NASA Office of Space Science via grant
NAG5-7584 and by other grants and contracts. IRAF, the Image Reduction
and Analysis Facility, is distributed by the National Optical Astronomy
Observatories, which are operated by the Association of Universities for
Research in Astronomy, Inc., under cooperative agreement with the
National Science Foundation. IDL is a registered trademark of Exelis
Visual Information Solutions, Inc., for its Interactive Data Language
software.
NR 17
TC 2
Z9 2
U1 0
U2 1
PU UNIV CHICAGO PRESS
PI CHICAGO
PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA
SN 0004-6280
J9 PUBL ASTRON SOC PAC
JI Publ. Astron. Soc. Pac.
PD APR
PY 2013
VL 125
IS 926
BP 431
EP 443
DI 10.1086/670227
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 131BM
UT WOS:000317965800008
ER
PT J
AU Sonnett, S
Meech, K
Jedicke, R
Bus, S
Tonry, J
Hainaut, O
AF Sonnett, S.
Meech, K.
Jedicke, R.
Bus, S.
Tonry, J.
Hainaut, O.
TI Testing Accuracy and Precision of Existing Photometry Algorithms on
Moving Targets
SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF THE PACIFIC
LA English
DT Article
ID APERTURE PHOTOMETRY; CCD PHOTOMETRY; FIELDS; SEXTRACTOR; EXTRACTION;
NOISE; TOOL
AB Previous studies determining which astronomical photometry software is best suited for a particular dataset are usually focused on speed, source classification, and/or meeting a sensitivity requirement. For faint objects in particular, the priority is given to maximizing signal-to-noise ratio. Photometry of moving targets offers additional challenges (1) to aperture photometry because background object contamination varies from image to image, and (2) to routines that build a PSF model from point sources in the image because trailed field stars do not perfectly represent the PSF of the untrailed target. Here, we present the results of testing several photometry algorithms (tphot, DAOPHOT, DoPHOT, APT, and multiple techniques within Source Extractor and IRAF's PHOT) on data for a faint, slow-moving solar system object with a known light curve. We find that the newly-developed tphot software most accurately and precisely reproduces the object's true light curve, with particular advantages in centroiding, exclusion of contaminants from the target's flux, and fitting flux in the wings of the point-spread function.
C1 [Sonnett, S.; Meech, K.; Jedicke, R.; Bus, S.; Tonry, J.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA.
[Sonnett, S.; Meech, K.] Univ Hawaii, NASA, Astrobiol Inst, Honolulu, HI 96822 USA.
[Hainaut, O.] European So Observ, D-85748 Garching, Germany.
RP Sonnett, S (reprint author), Univ Hawaii, Inst Astron, 2680 Woodlawn Dr, Honolulu, HI 96822 USA.
FU National Aeronautics and Space Administration by NASA [NAG5-4495,
NNX07A044G, NNX07AF79G]; National Science Foundation [AST-1010059,
AST-1009749]
FX This material is based upon work supported by the National Aeronautics
and Space Administration by NASA Grant Nos. NAG5-4495, NNX07A044G,
NNX07AF79G, and from the National Science Foundation through grant
AST-1010059. Partial support for this work was provided by National
Science Foundation grant AST-1009749. Initial image processing in this
article has been performed using the IRAF software. IRAF is distributed
by the National Optical Astronomy Observatories, which is operated by
the Association of Universities for Research in Astronomy, Inc. (AURA)
under cooperative agreement with the National Science Foundation.
NR 25
TC 1
Z9 1
U1 0
U2 0
PU UNIV CHICAGO PRESS
PI CHICAGO
PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA
SN 0004-6280
J9 PUBL ASTRON SOC PAC
JI Publ. Astron. Soc. Pac.
PD APR
PY 2013
VL 125
IS 926
BP 456
EP 469
DI 10.1086/670593
PG 14
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 131BM
UT WOS:000317965800010
ER
PT J
AU El Akkraoui, A
Tremolet, Y
Todling, R
AF El Akkraoui, Amal
Tremolet, Yannick
Todling, Ricardo
TI Preconditioning of variational data assimilation and the use of a
bi-conjugate gradient method
SO QUARTERLY JOURNAL OF THE ROYAL METEOROLOGICAL SOCIETY
LA English
DT Article
DE minimization algorithms; Lanczos method; 4D-Var; GSI; preconditioned
Conjugate Gradient methods
ID ECMWF OPERATIONAL IMPLEMENTATION; NONSYMMETRIC LINEAR-SYSTEMS;
METEOROLOGICAL OBSERVATIONS; 4D-VAR; MODEL; CONVERGENCE; SCHEME;
COVARIANCES; ALGORITHMS; EQUATIONS
AB Presently, a preferred minimization for strong-constraint four-dimensional variational (4D-Var) assimilation uses a Lanczos-based conjugate gradient (CG) algorithm. This requires the availability of a square-root of the background-error covariance matrix (B). In the context of weak-constraint 4D-Var, this requirement might be too restrictive for the formulations of the model error term. It might therefore be desirable to avoid a square-root decomposition of the augmented background term. An appealing minimization scheme is the double CG minimization employed, for example, in the grid-point statistical interpolation (GSI) analysis. Realizing the double CG algorithm is a special case of the more general bi-conjugate gradient (BiCG) method for solving non-symmetric problems, the present work introduces a Lanczos-based preconditioning strategy when B, instead of its square-root, is used initially. Implementation of the scheme is done in the context of the GSI analysis system, and preliminary experiments are presented using its 3D-Var version. Comparison of the Lanczos-based CG and the BiCG shows that the algorithms converge at the same rate and to the same solution. Despite the additional computational cost, the importance of the re-orthogonalization step is also shown to be fundamental to any of these CG algorithms. Furthermore, when using the Hessian eigenvectors for preconditioning, the BiCG behaviour is shown to be comparable to that of the Lanczos-CG algorithm. Both schemes construct the same approximation of the Hessian with the same number of eigenvectors, and benefit in the same way from the reduction of the condition number. The efficiency, computational cost, and stability of the three algorithms are discussed. Copyright (c) 2012 Royal Meteorological Society
C1 [El Akkraoui, Amal; Todling, Ricardo] NASA, Global Modeling & Assimilat Off, Greenbelt, MD 20771 USA.
[El Akkraoui, Amal] Sci Syst & Applicat Inc, Lanham, MD USA.
[Tremolet, Yannick] European Ctr Medium Range Weather Forecasts, Reading RG2 9AX, Berks, England.
RP El Akkraoui, A (reprint author), NASA, Global Modeling & Assimilat Off, GSFC, Code 610-1, Greenbelt, MD 20771 USA.
EM amal.elakkraoui@nasa.gov
NR 50
TC 5
Z9 5
U1 0
U2 4
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 0035-9009
J9 Q J ROY METEOR SOC
JI Q. J. R. Meteorol. Soc.
PD APR
PY 2013
VL 139
IS 672
BP 731
EP 741
DI 10.1002/qj.1997
PN A
PG 11
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 130QK
UT WOS:000317933600013
ER
PT J
AU Whitehurst, AS
Swatantran, A
Blair, JB
Hofton, MA
Dubayah, R
AF Whitehurst, Amanda S.
Swatantran, Anu
Blair, J. Bryan
Hofton, Michelle A.
Dubayah, Ralph
TI Characterization of Canopy Layering in Forested Ecosystems Using Full
Waveform Lidar
SO REMOTE SENSING
LA English
DT Article
DE lidar; vertical structure; canopy layering; New Hampshire
ID DISCRETE-RETURN LIDAR; SPECIES-DIVERSITY; AIRBORNE LIDAR; TREE GROWTH;
RAIN-FOREST; STRUCTURAL CHARACTERISTICS; LASER ALTIMETER; TROPICAL
FOREST; SMALL-FOOTPRINT; VEGETATION
AB Canopy structure, the vertical distribution of canopy material, is an important element of forest ecosystem dynamics and habitat preference. Although vertical stratification, or "canopy layering," is a basic characterization of canopy structure for research and forest management, it is difficult to quantify at landscape scales. In this paper we describe canopy structure and develop methodologies to map forest vertical stratification in a mixed temperate forest using full-waveform lidar. Two definitions-one categorical and one continuous-are used to map canopy layering over Hubbard Brook Experimental Forest, New Hampshire with lidar data collected in 2009 by NASA's Laser Vegetation Imaging Sensor (LVIS). The two resulting canopy layering datasets describe variation of canopy layering throughout the forest and show that layering varies with terrain elevation and canopy height. This information should provide increased understanding of vertical structure variability and aid habitat characterization and other forest management activities.
C1 [Whitehurst, Amanda S.; Swatantran, Anu; Hofton, Michelle A.; Dubayah, Ralph] Univ Maryland, Dept Geog Sci, College Pk, MD 20742 USA.
[Blair, J. Bryan] NASA, Goddard Space Flight Ctr, Laser Remote Sensing Lab, Greenbelt, MD 20771 USA.
RP Whitehurst, AS (reprint author), Univ Maryland, Dept Geog Sci, 2181 Samuel J LeFrak Hall, College Pk, MD 20742 USA.
EM awhitehu@umd.edu; aswatan@umd.edu; james.b.blair@nasa.gov;
mhofton@umd.edu; dubayah@umd.edu
RI Blair, James/D-3881-2013; Beckley, Matthew/D-4547-2013; Swatantran,
Anu/B-8786-2016
FU NASA Graduate Student Researchers Program Fellowship [NNX09AL43H]
FX We would like to thank Geoffrey Parker, Sean McMahon, and Eric Kasischke
for their conceptual advice and comments throughout the research
process. Also, we would like to thank Naiara Pinto and Joseph Sexton for
their editorial reviews of this manuscript and Jyoteshwar Nagol for his
technical expertise. This project was funded by the NASA Graduate
Student Researchers Program Fellowship, grant number NNX09AL43H.
NR 60
TC 17
Z9 18
U1 1
U2 50
PU MDPI AG
PI BASEL
PA POSTFACH, CH-4005 BASEL, SWITZERLAND
SN 2072-4292
J9 REMOTE SENS-BASEL
JI Remote Sens.
PD APR
PY 2013
VL 5
IS 4
BP 2014
EP 2036
DI 10.3390/rs5042014
PG 23
WC Remote Sensing
SC Remote Sensing
GA 131TZ
UT WOS:000318020600025
ER
PT J
AU James, JT
Lam, CW
Santana, PA
Scully, RR
AF James, John T.
Lam, Chiu-Wing
Santana, Patricia A.
Scully, Robert R.
TI Estimate of safe human exposure levels for lunar dust based on
comparative benchmark dose modeling
SO INHALATION TOXICOLOGY
LA English
DT Article
DE Benchmark dose; inhalation; lunar dust; mineral dust
ID TOXICITY
AB Brief exposures of Apollo astronauts to lunar dust occasionally elicited upper respiratory irritation; however, no limits were ever set for prolonged exposure to lunar dust. The United States and other space faring nations intend to return to the moon for extensive exploration within a few decades. In the meantime, habitats for that exploration, whether mobile or fixed, must be designed to limit human exposure to lunar dust to safe levels. Herein we estimate safe exposure limits for lunar dust collected during the Apollo 14 mission. We instilled three respirable- sized (similar to 2 mu mass median diameter) lunar dusts (two ground and one unground) and two standard dusts of widely different toxicities (quartz and TiO2) into the respiratory system of rats. Rats in groups of six were given 0, 1, 2.5 or 7.5 mg of the test dust in a saline-Survanta (R) vehicle, and biochemical and cellular biomarkers of toxicity in lung lavage fluid were assayed 1 week and one month after instillation. By comparing the dose-response curves of sensitive biomarkers, we estimated safe exposure levels for astronauts and concluded that unground lunar dust and dust ground by two different methods were not toxicologically distinguishable. The safe exposure estimates were 1.3 +/- 0.4 mg/m(3) (jet-milled dust), 1.0 +/- 0.5 mg/m(3) (ball-milled dust) and 0.9 +/- 0.3 mg/m(3) (unground, natural dust). We estimate that 0.5-1 mg/ m(3) of lunar dust is safe for periodic human exposures during long stays in habitats on the lunar surface.
C1 [James, John T.] NASA, Lyndon B Johnson Space Ctr, Space Toxicol Off, Houston, TX 77058 USA.
[Lam, Chiu-Wing; Scully, Robert R.] Wyle Sci Technol & Engn Grp, Houston, TX USA.
[Santana, Patricia A.] Univ Space Res Assoc, Houston, TX USA.
RP James, JT (reprint author), NASA, Lyndon B Johnson Space Ctr, Space Toxicol Off, Houston, TX 77058 USA.
EM john.t.james@nasa.gov
FU Human Research Program of the NASA
FX This work was supported by the Human Research Program of the NASA. The
estimates provided herein should not be construed as official NASA
standards. The conclusions are those of the authors alone, and we report
no conflicts of interest.
NR 10
TC 4
Z9 4
U1 0
U2 8
PU INFORMA HEALTHCARE
PI LONDON
PA TELEPHONE HOUSE, 69-77 PAUL STREET, LONDON EC2A 4LQ, ENGLAND
SN 0895-8378
J9 INHAL TOXICOL
JI Inhal. Toxicol.
PD APR
PY 2013
VL 25
IS 5
BP 243
EP 256
DI 10.3109/08958378.2013.777821
PG 14
WC Toxicology
SC Toxicology
GA 131YJ
UT WOS:000318034500002
PM 23614726
ER
PT J
AU Chatterjee, A
Plawsky, JL
Wayner, PC
Chao, DF
Sicker, RJ
Lorik, T
Chestney, L
Margie, R
Eustace, J
Zoldak, J
AF Chatterjee, Arya
Plawsky, Joel L.
Wayner, Peter C., Jr.
Chao, David F.
Sicker, Ronald J.
Lorik, Tibor
Chestney, Louis
Margie, Raymond
Eustace, John
Zoldak, John
TI Constrained Vapor Bubble Heat Pipe Experiment Aboard the International
Space Station
SO JOURNAL OF THERMOPHYSICS AND HEAT TRANSFER
LA English
DT Article; Proceedings Paper
CT 49th AIAA Aerospace Sciences Meeting including the New Horizons Forum
and Aerospace Exposition
CY JAN 03-07, 2011
CL Orlando, FL
SP AIAA
ID TRIANGULAR MICROGROOVES; PREDICTION; TRANSPORT; EXCHANGER; GROOVES; FIN
AB A constrained vapor bubble heat pipe experiment was run in the microgravity environment of the International Space Station. Here we present the initial results that demonstrate significant differences in the operation of the constrained vapor bubble heat pipe in the microgravity environment as compared to the Earth's gravity. The temperature profile data along the heat pipe indicate that the heat pipe behavior is affected favorably by increased capillary flow and adversely by the absence of outside convective heat transfer as a heat loss mechanism. The reflectivity pattern viewed through the transparent quartz wall documented complex microflow patterns. Image data of the liquid profile in the grooves of the heat pipe indicate that the curvature gradient giving capillary flow is considerably different from that on Earth. Using experimental data for the temperature and meniscus profiles, a one-dimensional model gives the inside heat transfer coefficient, which was significantly higher in microgravity. An initial discussion of some of the data collected is presented.
C1 [Chatterjee, Arya; Plawsky, Joel L.; Wayner, Peter C., Jr.] Rensselaer Polytech Inst, Troy, NY 12180 USA.
[Chao, David F.; Sicker, Ronald J.] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA.
[Lorik, Tibor; Chestney, Louis; Margie, Raymond; Eustace, John; Zoldak, John] Zin Technol, Cleveland, OH 44130 USA.
RP Plawsky, JL (reprint author), Rensselaer Polytech Inst, Troy, NY 12180 USA.
EM arya.chatterjee@gmail.com; plawsky@rpi.edu; wayner@rpi.edu;
david.f.chao@nasa.gov; ronald.j.sicker@nasa.gov; lorikt@ZIN-TECH.COM;
ChestneyL@ZIN-TECH.COM; margier@Zin-tech.com; eustacej@ZIN-TECH.COM;
zoldakj@ZIN-TECH.COM
NR 23
TC 9
Z9 9
U1 0
U2 19
PU AMER INST AERONAUTICS ASTRONAUTICS
PI RESTON
PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA
SN 0887-8722
EI 1533-6808
J9 J THERMOPHYS HEAT TR
JI J. Thermophys. Heat Transf.
PD APR-JUN
PY 2013
VL 27
IS 2
BP 309
EP 319
DI 10.2514/1.T3792
PG 11
WC Thermodynamics; Engineering, Mechanical
SC Thermodynamics; Engineering
GA 129YT
UT WOS:000317880600011
ER
PT J
AU Glaze, LS
Baloga, SM
AF Glaze, Lori S.
Baloga, Stephen M.
TI Simulation of inflated pahoehoe lava flows
SO JOURNAL OF VOLCANOLOGY AND GEOTHERMAL RESEARCH
LA English
DT Article
DE Lava flows; Pahoehoe; Modeling; Simulation
ID KILAUEA VOLCANO; INCLINED PLANE; FLOOD LAVAS; RANDOM-WALK; HAWAII;
MODEL; EMPLACEMENT; EXAMPLES; TUMULI; MARS
AB A new stochastic model simulates late-stage pahoehoe lobes where random processes dominate emplacement. The model prescribes probabilistic rules for determining where and when parcels of lava move within the lobe. Unlike a classical Brownian motion random walk, the model allows individual parcels to remain dormant, but fluid, for multiple time steps. The randomness of parcel volume transfers within the lobe interior as well as at the margins qualitatively reflects inflation processes observed in the field. The fraction of inflated volume to total volume increases with the total volume, with greater than 75% of the lobe volume contributed through inflation for typical lobes. The influence on planform shape and topographic cross-sectional profiles of total volume, source area and shape, topographic confinement, and sequential breakouts at the lobe margins, are all explored with the stochastic model. Each of these factors influences the overall lobe thickness and width. The model provides a means for assessing the relative importance of these processes through comparisons with field data. For the first time, Gaussian and parabolic functions are quantitatively fit to field measurements of pahoehoe lobes. Both functional forms provide adequate description of the cross-sectional flow shapes. When comparing simulated lobes to field data, sequential breakouts at the lobe margins are found to be an important process controlling the final topographic distribution of observed pahoehoe lobes. (C) 2013 Published by Elsevier B.V.
C1 [Glaze, Lori S.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Baloga, Stephen M.] Proxemy Res, Gaithersburg, MD 20882 USA.
RP Glaze, LS (reprint author), NASA, Goddard Space Flight Ctr, Code 698,8800 Greenbelt Rd, Greenbelt, MD 20771 USA.
EM Lori.S.Glaze@nasa.gov; steve@proxemy.com
RI Glaze, Lori/D-1314-2012
FU NASA [WBS 811073.02.01.04.44, NNX08AF16G, WBS 203959.02.03.17.56,
NNX10AP63G]
FX This work was funded by the NASA Planetary Geology and Geophysics
Program (WBS 811073.02.01.04.44 for L. Glaze, and grant NNX08AF16G for
S. Baloga) and the NASA Mars Data Analysis Program (WBS
203959.02.03.17.56 for L Glaze, and grant NNX10AP63G for S. Baloga). The
authors would like to thank Dr. Scott Rowland for many insightful
discussions in the field over a number of years and Dr. Christopher
Hamilton for helpful comments on this manuscript and discussions of
quantitative field observations. Many others have also contributed over
many years regarding basic behavior of pahoehoe lava flows, including S.
Self, A. Harris, T. Thordarson, J. Bleacher, and R. Wright. L. Kestay
and an anonymous reviewer kindly provided very helpful comments on this
manuscript.
NR 38
TC 4
Z9 4
U1 1
U2 10
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0377-0273
EI 1872-6097
J9 J VOLCANOL GEOTH RES
JI J. Volcanol. Geotherm. Res.
PD APR 1
PY 2013
VL 255
BP 108
EP 123
DI 10.1016/j.jvolgeores.2013.01.018
PG 16
WC Geosciences, Multidisciplinary
SC Geology
GA 126PQ
UT WOS:000317633800009
ER
PT J
AU Liang, ZB
He, ZL
Zhou, XX
Powell, CA
Yang, YG
He, LM
Stoffella, PJ
AF Liang, Zhanbei
He, Zhenli
Zhou, Xuxia
Powell, Charles A.
Yang, Yuangen
He, Li Ming
Stoffella, Peter J.
TI Impact of mixed land-use practices on the microbial water quality in a
subtropical coastal watershed
SO SCIENCE OF THE TOTAL ENVIRONMENT
LA English
DT Article
DE Surface runoff water; Fecal indicator bacteria; Salmonella; Land use;
Host specific marker; Environmental parameters
ID FECAL INDICATOR BACTERIA; ESCHERICHIA-COLI; SOUTH FLORIDA; PCR ASSAY;
POLLUTION; SALMONELLA; CONTAMINATION; STREAM; ASSOCIATIONS; PERSISTENCE
AB Surface runoff water is an important non-point source of fecal pollution to downstream water; however, there is a lack of systematic studies on the microbial quality of surface runoff water from watersheds with mixed land uses. In this study water samples from 12 surface runoff holding water bodies (SRW), which collected runoff from various patterns of land use within the St. Lucie watershed along the southeastern coastline of Florida, were collected monthly for 22 months. The concentration of fecal indicator bacteria (FIB) and frequency of detection of Salmonella and host specific markers (HF183, CF128, CF193, and HS-esp) were determined, and their associations with land use, rainfall, and water physico-chemical parameters were investigated. Higher FIB concentrations were observed from urban land and cattle ranch sites. Within the same primary land use pattern, different sub-patterns did not have the same level of FIB: golf communities contributed less to fecal pollution than residential areas, and plant nursery sites contained relative higher FIB concentrations than other agricultural sites. Salmonella, CF128, and CF193 markers were more frequently detected from the cattle ranch sites. In contrast the frequency of detecting human specific markers (HF183 and HS-esp) was much higher in residential sites. Rainfall positively affected the concentration of FIB and occurrence of Salmonella, possibly by providing more inputs or mobilizing the sources from sediments. Water temperature, dissolved organic carbon (DOC), and nutrient levels were positively correlated with FIB concentrations and occurrence in SRW, possibly by promoting their growth and survival. This study indicated the need for site specific mitigation strategies to improve SRW and downstream water quality. (C) 2013 Elsevier B.V. All rights reserved.
C1 [Liang, Zhanbei; He, Zhenli; Zhou, Xuxia; Powell, Charles A.; Yang, Yuangen; Stoffella, Peter J.] Univ Florida, Inst Food & Agr Sci, Indian River Res & Educ Ctr, Ft Pierce, FL 34945 USA.
[He, Li Ming] NOAA, Natl Marine Fisheries Serv, Sacramento, CA 95814 USA.
RP He, ZL (reprint author), Univ Florida, Inst Food & Agr Sci, Indian River Res & Educ Ctr, Ft Pierce, FL 34945 USA.
EM lzbei001@gmail.com; zhe@ufl.edu; zhouxx1205@163.com; capowell@ufl.edu;
ygyang@ufl.edu; li-ming.he@noaa.gov; pjs@ufl.edu
RI He, Zhenli/R-1494-2016
OI He, Zhenli/0000-0001-7761-2070
FU South Florida Water Management District [4600001774]; GIS
FX This study was in part supported by a grant (contract#4600001774) from
South Florida Water Management District. Authors acknowledge Dr.
Chonggang Xu for GIS support. Special thanks are extended to anonymous
reviewers whose comments improved the manuscript.
NR 52
TC 15
Z9 15
U1 3
U2 45
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0048-9697
J9 SCI TOTAL ENVIRON
JI Sci. Total Environ.
PD APR 1
PY 2013
VL 449
BP 426
EP 433
DI 10.1016/j.scitotenv.2013.01.087
PG 8
WC Environmental Sciences
SC Environmental Sciences & Ecology
GA 125KH
UT WOS:000317538200049
PM 23454704
ER
PT J
AU Liu, YQ
Peters-Lidard, CD
Kumar, S
Foster, JL
Shaw, M
Tian, YD
Fall, GM
AF Liu, Yuqiong
Peters-Lidard, Christa D.
Kumar, Sujay
Foster, James L.
Shaw, Michael
Tian, Yudong
Fall, Gregory M.
TI Assimilating satellite-based snow depth and snow cover products for
improving snow predictions in Alaska
SO ADVANCES IN WATER RESOURCES
LA English
DT Article
DE Data assimilation; Satellite snow products; Snow prediction; Streamflow
prediction
ID ENSEMBLE KALMAN FILTER; LAND INFORMATION-SYSTEM; HYDROLOGY MODEL;
SURFACE MODEL; MODIS; FRAMEWORK; AREA
AB Several satellite-based snow products are assimilated, both separately and jointly, into the Noah land surface model for improving snow prediction in Alaska. These include the standard and interpreted versions of snow cover fraction (SCF) data from the Moderate-Resolution Imaging Spectroradiometer (MODIS) and the snow depth (SD) estimates from the Advanced Microwave Scanning Radiometer for the Earth Observing System (AMSR-E). The satellite-based SD estimates are adjusted against in situ observations via statistical interpolation to reduce the potentially large biases, prior to being assimilated using an ensemble Kalman filter. A customized, rule-based direct insertion approach is developed to assimilate the two SCF datasets. Our results indicate that considerable overall improvement on snow prediction can be achieved via assimilating the bias-adjusted satellite SD estimates; however, the improvement does not always translate into improvements in streamflow prediction. Assimilating the standard MODIS SCF is found to have little impact on snow and streamflow predictions, while assimilating the interpreted SCF estimates, which have reduced cloud coverage and improved snow mapping accuracy, has resulted in the most consistent improvements on snow and streamflow predictions across the study domain. (C) 2013 Elsevier Ltd. All rights reserved.
C1 [Liu, Yuqiong; Kumar, Sujay; Tian, Yudong] Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20742 USA.
[Liu, Yuqiong; Peters-Lidard, Christa D.; Foster, James L.; Shaw, Michael; Tian, Yudong] NASA, Hydrol Sci Lab, Goddard Space Flight Ctr, Greenbelt, MD USA.
[Kumar, Sujay; Shaw, Michael] Sci Applicat Int Corp, Beltsville, MD USA.
[Shaw, Michael] AF Weather Agcy, Offutt, NE USA.
[Fall, Gregory M.] Natl Operat Hydrol Remote Sensing Ctr, Chanhassem, MN USA.
RP Liu, YQ (reprint author), Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20742 USA.
EM Yuqiong.Liu@nasa.gov
RI Kumar, Sujay/B-8142-2015; Peters-Lidard, Christa/E-1429-2012
OI Peters-Lidard, Christa/0000-0003-1255-2876
FU NASA [NNX08AU51G]; NASA; NOAA; Air Force Weather Agency (AFWA)
FX Support for this study was provided by NASA under Grant NNX08AU51G and
as part of NASA's contribution to the National Climate Assessment
program. Additional funding comes from NOAA and the Air Force Weather
Agency (AFWA). Comments from Martyn Clark and an anonymous reviewer
helped to improve this manuscript.
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PU ELSEVIER SCI LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND
SN 0309-1708
J9 ADV WATER RESOUR
JI Adv. Water Resour.
PD APR
PY 2013
VL 54
BP 208
EP 227
DI 10.1016/j.advwatres.2013.02.005
PG 20
WC Water Resources
SC Water Resources
GA 122UT
UT WOS:000317344300015
ER
PT J
AU Arzeno, NM
Stenger, MB
Lee, SMC
Ploutz-Snyder, R
Platts, SH
AF Arzeno, Natalia M.
Stenger, Michael B.
Lee, Stuart M. C.
Ploutz-Snyder, Robert
Platts, Steven H.
TI Sex differences in blood pressure control during 6 degrees head-down
tilt bed rest
SO AMERICAN JOURNAL OF PHYSIOLOGY-HEART AND CIRCULATORY PHYSIOLOGY
LA English
DT Article
DE microgravity; spaceflight; heart rate variability; autonomic control;
baroreflex sensitivity
ID AUTONOMIC CARDIOVASCULAR REGULATION; SYMPATHETIC-NERVE ACTIVITY;
PLASMA-VOLUME RESTORATION; RATE-VARIABILITY; BAROREFLEX SENSITIVITY;
ORTHOSTATIC HYPOTENSION; GENDER-DIFFERENCES; ARTERIAL-PRESSURE;
MENSTRUAL-CYCLE; CARDIAC BAROREFLEX
AB Arzeno NM, Stenger MB, Lee SM, Ploutz-Snyder R, Platts SH. Sex differences in blood pressure control during 6 degrees head-down tilt bed rest. Am J Physiol Heart Circ Physiol 304: H1114-H1123, 2013. First published February 8, 2013; doi: 10.1152/ajpheart.00391.2012.-Spaceflight-induced orthostatic intolerance has been studied for decades. Although similar to 22% of the astronaut corps are women, most mechanistic studies use mostly male subjects, despite known sex differences in autonomic control and postflight orthostatic intolerance. We studied adrenergic, baroreflex, and autonomic indexes during continuous infusions of vasoactive drugs in men and women during a 60-day head-down bed rest. Volunteers were tested before bed rest (20 men and 10 women) and around day 30 (20 men and 10 women) and day 60 (16 men and 8 women) of bed rest. Three increasing doses of phenylephrine (PE) and sodium nitroprusside were infused for 10 min after an infusion of normal saline. A 20-min rest period separated the phenylephrine and sodium nitroprusside infusions. Autonomic activity was approximated by spectral indexes of heart rate and blood pressure variability, and baroreflex sensitivity was measured by the spontaneous baroreflex slope. Parasympathetic modulation and baroreflex sensitivity decreased with bed rest, with women experiencing a larger decrease in baroreflex sensitivity by day 30 than men. The sympathetic activation of men and parasympathetic responsiveness of women in blood pressure control during physiological stress were preserved throughout bed rest. During PE infusions, women experienced saturation of the R-R interval at high frequency, whereas men did not, revealing a sex difference in the parabolic relationship between high-frequency R-R interval, a measurement of respiratory sinus arrhythmia, and R-R interval. These sex differences in blood pressure control during simulated microgravity reveal the need to study sex differences in long-duration spaceflight to ensure the health and safety of the entire astronaut corps.
C1 [Arzeno, Natalia M.; Stenger, Michael B.; Lee, Stuart M. C.] Wyle Sci Technol & Engn Grp, Houston, TX USA.
[Ploutz-Snyder, Robert] Univ Space Res Assoc, Houston, TX USA.
[Platts, Steven H.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA.
RP Stenger, MB (reprint author), 1290 Hercules Dr, Houston, TX 77058 USA.
EM michael.b.stenger@nasa.gov
FU National Aeronautics and Space Administration (NASA)
[BRC-2003-0000-0543]; NASA Flight Analogs Project; NCRR [M01-RR-0073]
FX This work was funded by National Aeronautics and Space Administration
(NASA) Grant BRC-2003-0000-0543 and sponsored by the NASA Flight Analogs
Project. This work was conducted at the National Center for Research
Resources (NCRR)-funded (NCRR Grant M01-RR-0073) General Clinical
Research Center at the University of Texas Medical Branch (Galveston,
TX).
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PU AMER PHYSIOLOGICAL SOC
PI BETHESDA
PA 9650 ROCKVILLE PIKE, BETHESDA, MD 20814 USA
SN 0363-6135
J9 AM J PHYSIOL-HEART C
JI Am. J. Physiol.-Heart Circul. Physiol.
PD APR
PY 2013
VL 304
IS 8
BP H1114
EP H1123
DI 10.1152/ajpheart.00391.2012
PG 10
WC Cardiac & Cardiovascular Systems; Physiology; Peripheral Vascular
Disease
SC Cardiovascular System & Cardiology; Physiology
GA 126GP
UT WOS:000317601600008
PM 23396455
ER
PT J
AU Righter, K
Danielson, LR
Pando, K
Morris, RV
Graff, TG
Agresti, DG
Martin, AM
Sutton, SR
Newville, M
Lanzirotti, A
AF Righter, Kevin
Danielson, Lisa R.
Pando, Kellye
Morris, Richard V.
Graff, Trevor G.
Agresti, David G.
Martin, Audrey M.
Sutton, Stephen R.
Newville, Matt
Lanzirotti, Antonio
TI Redox systematics of martian magmas with implications for magnetite
stability
SO AMERICAN MINERALOGIST
LA English
DT Article
DE Mars; basalt; redox; magnetite
ID NATURAL SILICATE LIQUIDS; MARS MOSSBAUER DATA; OXIDATION-STATE; OXYGEN
FUGACITY; MELT EQUILIBRIA; SNC METEORITES; FREE-ENERGY; IRON;
SHERGOTTITE; CRYSTALLIZATION
AB Magnetite is commonly found at sites on Mars explored by robotic spacecraft, yet is rare in martian meteorites and in experimental studies of martian magma compositions. Iron redox systematics of the high-FeO shergottitic liquids are poorly known, yet have a fundamental control on stability of phases such as magnetite, ilmenite, and pyroxenes. We undertook experiments to constrain the Fe3+/Sigma Fe in high-FeO (15-22 wt%) glasses as a function of f(O2), melt P2O5, temperature and pressure. We also performed a series of sub-liquidus experiments between 1100 and 1000 degrees C and FMQ+0.5 to FMQ-1 to define magnetite stability. Run products were analyzed for Fe3+ and Fe2+ by Mossbauer spectroscopy and micro-X-ray absorption near edge structure (micro-XANES) spectroscopy. One bar liquids equilibrated at FMQ-3 to FMQ+3 show a much lower Fe3+/Sigma Fe than terrestrial basalts at the same conditions. As melt P2O5 contents increase from 0 to 3 wt% (at fixed pressure, temperature, and f(O2)), Fe3+/Sigma Fe decreases from 0.07 to 0.05, but this is within error on the measurements. Temperature increases between 1200 and 1500 degrees C cause little to no variation in Fe3+/Sigma Fe. Pressure increases from 1 to 4 GPa cause a 0.06 decrease in Fe3+/Sigma Fe. The trends with pressure and temperature are in agreement with results of previous studies. Combining our new series of data allows derivation of an expression to calculate Fe3+/Fe2+ for high-FeO melts such as martian magmas.
ln(XFe3+/XFe2+) = a lnf(O2) + b/T + cP/T + dX(FeO) + eX(Al2O3) + fX(CaO) + gX(Na2O) + hX(K2O) + iX(P2O5) + j
This expression can be used to show that decompressed melts become slightly more oxidized at the surface (compared to 4 GPa). Magnetite stability is suppressed by the lower Fe3+/Fe2+ of the high-FeO melts. Magnetite stability is a function of Fe2O3 and temperature and is stable similar to 50 degrees C lower than typical terrestrial basalt. Difficulty in producing magnetite as a liquidus phase in magmatic systems suggests either that many martian basalts are more oxidized than FMQ (but not represented among meteorite collections), that the titano-magnetite only forms upon cooling below similar to 1000 degrees C at FMQ, or that the magnetite has a secondary origin.
C1 [Righter, Kevin; Morris, Richard V.; Martin, Audrey M.] NASA, Lyndon B Johnson Space Ctr, Mailcode KT, 2101 NASA Pkwy, Houston, TX 77058 USA.
[Danielson, Lisa R.; Pando, Kellye; Graff, Trevor G.] NASA, Engn & Sci Contract Grp, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA.
[Agresti, David G.] Univ Alabama Birmingham, Dept Phys, Birmingham, AL 35294 USA.
[Sutton, Stephen R.] Univ Chicago, Dept Geophys Sci, Chicago, IL 60637 USA.
[Sutton, Stephen R.; Newville, Matt; Lanzirotti, Antonio] Univ Chicago, Ctr Adv Radiat Sources, Chicago, IL 60637 USA.
RP Righter, K (reprint author), NASA, Lyndon B Johnson Space Ctr, Mailcode KT, 2101 NASA Pkwy, Houston, TX 77058 USA.
EM kevin.righter-1@nasa.gov
OI Martin, Audrey/0000-0002-1165-8866
FU NASA-JSC by an RTOP from the NASA Mars Fundamental Research program;
National Science Foundation-Earth Sciences [EAR-1128799]; Department of
Energy-Geosciences [DE-FG02-94ER14466]; U.S. Department of Energy,
Office of Science, Office of Basic Energy Sciences [DE-AC02-06CH11357]
FX We thank M. Toplis and T. McCoy for discussions relating to redox
equilibria in martian magmas, and to T. McCoy for loaning samples from
his experimental study. The journal reviews of J. Karner, G. Moore, and
D. Dyar helped to improve the clarity of the presentation of this
material. Loan Le provided assistance in the gas mixing furnace lab, and
Anne Peslier and Kent Ross provided assistance with the electron
microbeam analysis. This research was supported at NASA-JSC by an RTOP
to K.R. from the NASA Mars Fundamental Research program. Portions of
this work were performed at GeoSoilEnviroCARS (Sector 13), Advanced
Photon Source (APS), Argonne National Laboratory. GeoSoilEnviroCARS is
supported by the National Science Foundation-Earth Sciences
(EAR-1128799) and Department of Energy-Geosciences (DE-FG02-94ER14466).
Use of the Advanced Photon Source was supported by the U.S. Department
of Energy, Office of Science, Office of Basic Energy Sciences, under
Contract No. DE-AC02-06CH11357.
NR 71
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PU MINERALOGICAL SOC AMER
PI CHANTILLY
PA 3635 CONCORDE PKWY STE 500, CHANTILLY, VA 20151-1125 USA
SN 0003-004X
EI 1945-3027
J9 AM MINERAL
JI Am. Miner.
PD APR
PY 2013
VL 98
IS 4
BP 616
EP 628
DI 10.2138/am.2013.4251
PG 13
WC Geochemistry & Geophysics; Mineralogy
SC Geochemistry & Geophysics; Mineralogy
GA 123FG
UT WOS:000317373200011
ER
PT J
AU Shen, ZZ
Konishi, H
Brown, PE
Xu, HF
AF Shen, Zhizhang
Konishi, Hiromi
Brown, Philip E.
Xu, Huifang
TI STEM investigation of exsolution lamellae and "c" reflections in Ca-rich
dolomite from the Platteville Formation, western Wisconsin
SO AMERICAN MINERALOGIST
LA English
DT Article
DE Dolomite; Z-contrast imaging; Ca-Mg ordering; TEM; twinning; high
magnesian calcite; c-reflection; exsolution
ID CALCIAN DOLOMITE; MICROSTRUCTURES; SUPERSTRUCTURES; ANKERITE
AB Dolomite crystals in partially dolomitized limestone from the Platteville Formation are both compositionally and microstructurally heterogeneous. A single dolomite crystal usually contains three phases: the host Ca-rich dolomite [Ca1.14Mg0.86(CO3)(2)], an Fe-bearing dolomite [Ca1.06Mg0.80Fe0.14(CO3)(2)], and calcite inclusions. These three phases show similar orientations. The Ca-rich dolomite exhibits modulated microstructures with wavelength ranging from 7 to 30 nm. The modulated microstructures are not evident in Fe-bearing dolomite.
Modulations in the Ca-rich dolomite have three predominant orientation ranges in the studied sample: from (205) to (104), from (001) to ((1) over bar 01), and (110), which are consistent with previous studies. Bright-field (BF) and high-angle annular dark-field (HAADF) images confirm that these modulations are due to chemical variation rather than strain or diffraction contrast. The Ca-rich lamellae are Mg-rich calcite with compositions ranging from Ca0.85Mg0.15CO3 to Ca0.70Mg0.30CO3. The observed results indicate that these Ca-rich exsolution lamellae formed during diagenesis. In this study, three kinds of "c"-reflections, which are weak spots in the halfway position between the principal reflections along the (104)*, ((1) over bar 12)*, and (110)* directions, have been found in the diffraction patterns of some Ca-rich dolomite. Mg-Ca ordering in x-y planes was not observed directly in Z-contrast images. FFT patterns from the Z-contrast images do not show "c"-reflections. STEM images confirm that the "c"-reflections could result from multiple diffraction between the host dolomite and twinned Mg-calcite nano-lamellae under TEM imaging and diffraction modes.
C1 [Shen, Zhizhang; Konishi, Hiromi; Brown, Philip E.; Xu, Huifang] Univ Wisconsin, Dept Geosci, NASA Astrobiol Inst, Madison, WI 53706 USA.
RP Shen, ZZ (reprint author), Univ Wisconsin, Dept Geosci, NASA Astrobiol Inst, Madison, WI 53706 USA.
EM hfxu@geology.wisc.edu
FU NASA Astrobiology Institute [N07-5489]; NSF [EAR-095800]; U.S.
Department of Energy [DE-FG02-09ER16050]
FX This work is supported by NASA Astrobiology Institute (N07-5489), NSF
(EAR-095800), and U.S. Department of Energy (DE-FG02-09ER16050).
NR 20
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PU MINERALOGICAL SOC AMER
PI CHANTILLY
PA 3635 CONCORDE PKWY STE 500, CHANTILLY, VA 20151-1125 USA
SN 0003-004X
J9 AM MINERAL
JI Am. Miner.
PD APR
PY 2013
VL 98
IS 4
BP 760
EP 766
DI 10.2138/am.2013.4184
PG 7
WC Geochemistry & Geophysics; Mineralogy
SC Geochemistry & Geophysics; Mineralogy
GA 123FG
UT WOS:000317373200027
ER
PT J
AU Hilker, T
Frazer, GW
Coops, NC
Wulder, MA
Newnham, GJ
Stewart, JD
van Leeuwen, M
Culvenor, DS
AF Hilker, Thomas
Frazer, Gordon W.
Coops, Nicholas C.
Wulder, Michael A.
Newnham, Glenn J.
Stewart, James D.
van Leeuwen, Martin
Culvenor, Darius S.
TI Prediction of Wood Fiber Attributes from LiDAR-Derived Forest Canopy
Indicators
SO FOREST SCIENCE
LA English
DT Article
DE LiDAR; wood fiber; canopy structure; light regime; lodgepole pine
ID AIRBORNE LASER SCANNER; DOUGLAS-FIR; WESTERN HEMLOCK; MICROFIBRIL ANGLE;
PINUS-SYLVESTRIS; LODGEPOLE PINE; BASIC DENSITY; NORWAY SPRUCE; TREE
HEIGHT; SCOTS PINE
AB We investigated the potential use of airborne light detection and ranging (LiDAR) data to predict key wood fiber properties from extrinsic indicators in lodgepole pine leading forest stands located in the foothills of central Alberta, Canada. Six wood fiber attributes (wood density, cell perimeter, cell coarseness, mature fiber length, microfibril angle, and modulus of elasticity) were measured at 21 plots, and with use of data reduction techniques, two components of wood properties were derived: wood strength, stiffness, and fiber yield and fiber strength and smoothness. These wood fiber components were then compared with extrinsic indicators of wood characteristic-derived LiDAR-estimated topographic morphology, tree height, and canopy light metrics. The first principal component indicating wood strength and stiffness was significantly correlated to the depth of different canopy zones (or light regimes; r(2) = 0.55, P < 0.05). The second component, related to fiber strength and smoothness, was significantly correlated to the height of the canopy and canopy thickness (r(2) = 0.65, P < 0.05). The results indicate that airborne LiDAR attributes can explain about half of the observed variance in intrinsic wood fiber attributes, which is approximately 5-10% less than that explained by growth-related field-measured variables such as diameter increment and height. This reduction in explained variance can be balanced by the opportunities for much broader spatial characterizations of wood quantity and quality at the stand and landscape levels. FOR. SCI. 59(2):231-242.
C1 [Hilker, Thomas] Oregon State Univ, Coll Forestry, Corvallis, OR 97331 USA.
[Hilker, Thomas] NASA, Goddard Space Flight Ctr, Biospher Sci Branch, Greenbelt, MD 20771 USA.
[Frazer, Gordon W.; Wulder, Michael A.] Nat Resources Canada, Canadian Forest Serv, Ottawa, ON, Canada.
[Coops, Nicholas C.; van Leeuwen, Martin] Univ British Columbia, Vancouver, BC V5Z 1M9, Canada.
[Newnham, Glenn J.; Culvenor, Darius S.] CSIRO Land & Water, Black Mountain, ACT, Australia.
[Stewart, James D.] Nat Resources Canada, Canadian Wood Fiber Ctr, Ottawa, ON, Canada.
RP Hilker, T (reprint author), Oregon State Univ, Coll Forestry, Corvallis, OR 97331 USA.
EM thomas.hilker@oregonstate.edu
RI van Leeuwen, Martin/B-3947-2013; Coops, Nicholas/J-1543-2012; Newnham,
Glenn/G-8115-2011; Wulder, Michael/J-5597-2016;
OI van Leeuwen, Martin/0000-0003-2572-2088; Coops,
Nicholas/0000-0002-0151-9037; Wulder, Michael/0000-0002-6942-1896;
Stewart, James/0000-0003-1664-1083
FU Canadian Wood Fiber Centre of the Canadian Forest Service of Natural
Resources Canada; Natural Sciences and Engineering Research Council
FX We thank West Fraser Mills, Hinton Wood Products, for access to the
Integrated Wood Properties Trend Assessment wood quality and forest
inventory data sets. We are also grateful to Alberta Sustainable
Resource Development for access to the LiDAR data set. We thank Jared
Salvail and Prem Gurung (Canadian Wood Fiber Centre) for their
assistance in field plot location and measurements. The Canadian Wood
Fiber Centre of the Canadian Forest Service of Natural Resources Canada
provided funding to support this research with additional support from
an Natural Sciences and Engineering Research Council Discovery grant to
NC Coops.
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U1 2
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PU SOC AMER FORESTERS
PI BETHESDA
PA 5400 GROSVENOR LANE, BETHESDA, MD 20814 USA
SN 0015-749X
J9 FOREST SCI
JI For. Sci.
PD APR
PY 2013
VL 59
IS 2
BP 231
EP 242
PG 12
WC Forestry
SC Forestry
GA 123FJ
UT WOS:000317373500010
ER
PT J
AU Yi, TH
Zhang, GG
Tsujii, N
Fleurial, JP
Zevalkink, A
Snyder, GJ
Gronbech-Jensen, N
Kauzlarich, SM
AF Yi, Tanghong
Zhang, Gaigong
Tsujii, Naohito
Fleurial, Jean-Pierre
Zevalkink, Alex
Snyder, G. Jeffrey
Gronbech-Jensen, Niels
Kauzlarich, Susan M.
TI Phase Characterization, Thermal Stability, High-Temperature Transport
Properties, and Electronic Structure of Rare-Earth Zintl Phosphides
Eu3M2P4 (M = Ga, In)
SO INORGANIC CHEMISTRY
LA English
DT Article
ID THERMOELECTRIC PROPERTIES; CRYSTAL-STRUCTURE; BORON PHOSPHIDE; COMPOUND;
MAGNETORESISTANCE; EFFICIENCY; EU3IN2P4
AB Two rare-earth-containing ternary phosphides, Eu3Ga2P4 and Eu3In2P4, were synthesized by a two-step solid-state method with stoichiometric amounts of the constitutional elements. Refinements of the powder X-ray diffraction are consistent with the reported single-crystal structure with space group C2/c for Eu3Ga2P4 and Pnnm for Eu3In2P4. Thermal gravimetry and differential scanning calorimetry (TG-DSC) measurements reveal high thermal stability up to 1273 K. Thermal diffusivity measurements from room temperature to 800 K demonstrate thermal conductivity as low as 0.6 W/m.K for both compounds. Seebeck coefficient measurements from room temperature to 800 K indicate that both compounds are small band gap semiconductors. Eu3Ga2P4 shows p-type conductivity and Eu3In2P4 p-type conductivity in the temperature range 300-700 K and n-type conductivity above 700 K. Electronic structure calculations result in band gaps of 0.60 and 0.29 eV for Eu3Ga2P4 and Eu3In2P4, respectively. As expected for a valence precise Zintl phase, electrical resistivity is large, approximately 2600 and 560 m Omega.cm for Eu3Ga2P4 and Eu3In2P4 at room temperature, respectively. Measurements of transport properties suggest that these Zintl phosphides have potential for being good high-temperature thermoelectric materials with optimization of the charge carrier concentration by appropriate extrinsic dopants.
C1 [Yi, Tanghong; Tsujii, Naohito; Kauzlarich, Susan M.] Univ Calif Davis, Dept Chem, Davis, CA 95616 USA.
[Zhang, Gaigong; Gronbech-Jensen, Niels] Univ Calif Davis, Dept Appl Sci, Davis, CA 95616 USA.
[Tsujii, Naohito] Natl Inst Mat Sci, Tsukuba, Ibaraki 3050047, Japan.
[Fleurial, Jean-Pierre] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Zevalkink, Alex; Snyder, G. Jeffrey] CALTECH, Dept Mat Sci, Pasadena, CA 91109 USA.
RP Kauzlarich, SM (reprint author), Univ Calif Davis, Dept Chem, 1 Shields Ave, Davis, CA 95616 USA.
EM smkauzlarich@ucdavis.edu
RI Snyder, G. Jeffrey/E-4453-2011; Snyder, G/I-2263-2015; Tsujii,
Naohito/H-2544-2011
OI Snyder, G. Jeffrey/0000-0003-1414-8682; Tsujii,
Naohito/0000-0002-6181-5911
FU NSF [DMR1100313]; NSF/DOE [CBET-1048799]; NASA Jet Propulsion Laboratory
FX We gratefully acknowledge financial support from NSF DMR1100313, NSF/DOE
Partnership CBET-1048799, and NASA Jet Propulsion Laboratory.
NR 36
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U2 61
PU AMER CHEMICAL SOC
PI WASHINGTON
PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA
SN 0020-1669
EI 1520-510X
J9 INORG CHEM
JI Inorg. Chem.
PD APR 1
PY 2013
VL 52
IS 7
BP 3787
EP 3794
DI 10.1021/ic302400q
PG 8
WC Chemistry, Inorganic & Nuclear
SC Chemistry
GA 119JT
UT WOS:000317094300041
PM 23517094
ER
PT J
AU Navarrete, JU
Cappelle, IJ
Schnittker, K
Borrok, DM
AF Navarrete, Jesica U.
Cappelle, Ian J.
Schnittker, Kimberlin
Borrok, David M.
TI Bioleaching of ilmenite and basalt in the presence of iron-oxidizing and
iron-scavenging bacteria
SO INTERNATIONAL JOURNAL OF ASTROBIOLOGY
LA English
DT Article
DE Bioleaching; biomining; in situ resource utilization; iron oxidizing
bacteria; biomineral
ID PSEUDOMONAS-MENDOCINA; LEPTOSPIRILLUM-FERROOXIDANS;
THIOBACILLUS-FERROOXIDANS; DISSOLUTION KINETICS; MINERAL DISSOLUTION;
GROWTH; DRAINAGE; MOBILIZATION; METEORITES; SUPPORT
AB Bioleaching has been suggested as an alternative to traditional mining techniques in extraterrestrial environments because it does not require extensive infrastructure and bulky hardware. In situ bioleaching of silicate minerals, such as those found on the moon or Mars, has been proposed as a feasible alternative to traditional extraction techniques that require either extreme heat and/or substantial chemical treatment. In this study, we investigated the biotic and abiotic leaching of basaltic rocks (analogues to those found on the moon and Mars) and the mineral ilmenite (FeTiO3) in aqueous environments under acidic (pH similar to 2.5) and circumneutral pH conditions. The biological leaching experiments were conducted using Acidithiobacillus ferrooxidans, an iron (Fe)-oxidizing bacteria, and Pseudomonas mendocina, an Fe-scavenging bacteria. We found that both strains were able to grow using the Fe(II) derived from the tested basaltic rocks and ilmenite. Although silica leaching rates were the same or slightly less in the bacterial systems with A. ferrooxidans than in the abiotic control systems, the extent of Fe, Al and Ti released (and re-precipitated in new solid phases) was actually greater in the biotic systems. This is likely because the Fe(II) leached from the basalt was immediately oxidized by A. ferrooxidans, and precipitated into Fe(III) phases which causes a change in the equilibrium of the system, i.e. Le Chatelier's principle. Iron(II) in the abiotic experiment was allowed to build up in solution which led to a decrease in its overall release rate. For example, the percentage of Fe, Al and Ti leached (dissolved + reactive mineral precipitates) from the Mars simulant in the A. ferrooxidans experimental system was 34, 41 and 13% of the total Fe, Al and Ti in the basalt, respectively, while the abiotic experimental system released totals of only 11, 25 and 2%. There was, however, no measurable difference in the amounts of Fe and Ti released from ilmenite in the experiments with A. ferrooxidans versus the abiotic controls. P. mendocina scavenged some Fe from the rock/mineral substrates, but the overall amount of leaching was small (<2% of total Fe in rocks) when compared with the acidophilic systems. Although the mineralogy of the tested basaltic rocks was roughly similar, the surface areas of the lunar and Mars simulants varied greatly and thus were possible factors in the overall amount of metals released. Overall, our results indicate that the presence of bacteria does not increase the overall silica leaching rates of basaltic rocks; however, the presence of A. ferrooxidans does lead to enhanced release of Fe, Al and Ti and subsequent sequestration of Fe (and other metals) in Fe(III)-precipitates.
C1 [Navarrete, Jesica U.] Univ Calif Santa Cruz, Santa Cruz, CA 95064 USA.
[Navarrete, Jesica U.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Cappelle, Ian J.; Schnittker, Kimberlin; Borrok, David M.] Univ Texas El Paso, Dept Geol Sci, El Paso, TX 79968 USA.
RP Navarrete, JU (reprint author), Univ Calif Santa Cruz, Santa Cruz, CA 95064 USA.
EM jesica.u.navarrete@nasa.gov
FU NASA [NNX09AV09A]; Center for Space Exploration Research at The
University of Texas at El Paso; National Science Foundation Graduate
Research Fellowship Programme
FX The material is based upon work supported by NASA under award No.
NNX09AV09A and the Center for Space Exploration Research at The
University of Texas at El Paso. Graduate funding for J. Navarrete was
provided through the National Science Foundation Graduate Research
Fellowship Programme. In addition, we would like to thank Jose H. Garcia
of the Department of Geological Sciences at the University of Texas at
El Paso and Bonnie L. Cooper from the Astromaterials Research Group at
NASA Johnson Space Center for their assistance with the analysis of our
samples.
NR 39
TC 2
Z9 2
U1 0
U2 28
PU CAMBRIDGE UNIV PRESS
PI NEW YORK
PA 32 AVENUE OF THE AMERICAS, NEW YORK, NY 10013-2473 USA
SN 1473-5504
EI 1475-3006
J9 INT J ASTROBIOL
JI Int. J. Astrobiol.
PD APR
PY 2013
VL 12
IS 2
BP 123
EP 134
DI 10.1017/S1473550412000493
PG 12
WC Astronomy & Astrophysics; Biology; Geosciences, Multidisciplinary
SC Astronomy & Astrophysics; Life Sciences & Biomedicine - Other Topics;
Geology
GA 125FV
UT WOS:000317525900003
ER
PT J
AU Henderson, DS
L'Ecuyer, T
Stephens, G
Partain, P
Sekiguchi, M
AF Henderson, David S.
L'Ecuyer, Tristan
Stephens, Graeme
Partain, Phil
Sekiguchi, Miho
TI A Multisensor Perspective on the Radiative Impacts of Clouds and
Aerosols
SO JOURNAL OF APPLIED METEOROLOGY AND CLIMATOLOGY
LA English
DT Article
ID ENERGY SYSTEM CERES; BUDGET EXPERIMENT; CIRRUS CLOUDS; CLIMATE-RESEARCH;
MODIS; TOP; ATMOSPHERE; ISCCP; DISTRIBUTIONS; VALIDATION
AB The launch of CloudSat and Cloud-Aerosol Lidar and Infrared Pathfinder Satellite Observations (CALIPSO) in 2006 provided the first opportunity to incorporate information about the vertical distribution of cloud and aerosols directly into global estimates of atmospheric radiative heating. Vertical profiles of radar and lidar backscatter from CloudSat's Cloud Profiling Radar (CPR) and the Cloud-Aerosol Lidar with Orthogonal Polarization (CALIOP) aboard CALIPSO naturally complement Moderate Resolution Imaging Spectroradiometer (MODIS) radiance measurements, providing a nearly complete depiction of the cloud and aerosol properties that are essential for deriving high-vertical-resolution profiles of longwave (LW) and shortwave (SW) radiative fluxes and heating rates throughout the atmosphere. This study describes a new approach for combining vertical cloud and aerosol information from CloudSat and CALIPSO with MODIS data to assess impacts of clouds and aerosols on top-of-atmosphere (TOA) and surface radiative fluxes. The resulting multisensor cloud-aerosol product is used to document seasonal and annual mean distributions of cloud and aerosol forcing globally from June 2006 through April 2011. Direct comparisons with Clouds and the Earth's Radiant Energy System (CERES) TOA fluxes exhibit a close correlation, with improved errors relative to CloudSat-only products. Sensitivity studies suggest that remaining uncertainties in SW fluxes are dominated by uncertainties in CloudSat liquid water content estimates and that the largest sources of LW flux uncertainty are prescribed surface temperature and lower-tropospheric humidity. Globally and annually averaged net TOA cloud radiative effect is found to b -18.1 W m(-2). The global, annual mean aerosol direct radiative effect is found to be -1.6 +/- 0.5 W m(-2) (-2.5 +/- 0.8 W m(-2) if only clear skies over the ocean are considered), which, surprisingly, is more consistent with past modeling studies than with observational estimates that were based on passive sensors.
C1 [Henderson, David S.] Colorado State Univ, Dept Atmospher Sci, Ft Collins, CO 80523 USA.
[L'Ecuyer, Tristan] Univ Wisconsin, Dept Atmospher & Ocean Sci, Madison, WI USA.
[Stephens, Graeme] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Partain, Phil] Colorado State Univ, Cooperat Inst Res Atmosphere, Ft Collins, CO 80523 USA.
[Sekiguchi, Miho] Tokyo Univ Marine Sci & Technol, Tokyo, Japan.
RP Henderson, DS (reprint author), Colorado State Univ, 1371 Campus Delivery, Ft Collins, CO 80523 USA.
EM henderson@atmos.colostate.edu
RI L'Ecuyer, Tristan/C-7040-2013; L'Ecuyer, Tristan/E-5607-2012
OI L'Ecuyer, Tristan/0000-0002-7584-4836
FU NASA CloudSat Mission Grants [NAS5-99237, NASA JPL 1439268]
FX This research was supported by NASA CloudSat Mission Grants NAS5-99237
and NASA JPL 1439268. The authors thank the staff at the CloudSat Data
Processing Center (DPC) for their help in data processing. The authors
also thank Norm Wood and Colette Heald for assisting with CALIPSO data.
All CloudSat data presented here were acquired through the DPC and at
the time of writing could be accessed online
(http://www.cloudsat.cira.colostate.edu). CALIPSO data were obtained
online from the ASDC (http://eosweb.larc.nasa.gov).
NR 58
TC 36
Z9 36
U1 3
U2 47
PU AMER METEOROLOGICAL SOC
PI BOSTON
PA 45 BEACON ST, BOSTON, MA 02108-3693 USA
SN 1558-8424
J9 J APPL METEOROL CLIM
JI J. Appl. Meteorol. Climatol.
PD APR
PY 2013
VL 52
IS 4
BP 853
EP 871
DI 10.1175/JAMC-D-12-025.1
PG 19
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 128EX
UT WOS:000317753000008
ER
PT J
AU Yoo, JM
Won, YI
Jeong, MJ
Kim, KM
Shin, DB
Lee, YR
Cho, YJ
AF Yoo, Jung-Moon
Won, Young-In
Jeong, Myeong-Jae
Kim, Kyu-Myong
Shin, Dong-Bin
Lee, Yu-Ri
Cho, Young-Jun
TI Intensity of climate variability derived from the satellite and MERRA
reanalysis temperatures: AO, ENSO, and QBO
SO JOURNAL OF ATMOSPHERIC AND SOLAR-TERRESTRIAL PHYSICS
LA English
DT Article
DE MERRA; AMSU; Climate indices; AO; ENSO; QBO
ID LAND-SURFACE TEMPERATURE; EL-NINO; ARCTIC OSCILLATION; STRATOSPHERIC
TEMPERATURE; EXTRATROPICAL CIRCULATION; BAROCLINIC INSTABILITY;
SOUTHERN-OSCILLATION; BIENNIAL OSCILLATION; GROUND MEASUREMENTS;
CHANGING CLIMATE
AB Satellite measurements (Atmospheric InfraRed Sounder/Advanced Microwave Sounding Unit-A, MODerate resolution Imaging Spectroradiometer) and the Modern Era Retrospective-analysis for Research and Applications (MERRA) reanalysis have been utilized to analyze the relative influence of the climate variability (AO: Arctic Oscillation, ENSO: El Nino-Southern Oscillation, QBO: Quasi-Biennial Oscillation) on the zonal-mean temperature and wind variations over the globe from September 2002 to August 2011. We also extended the usage of MERRA data for the period of 1979-2011; furthermore, three climate indices of AO, NINO3.4, and QBO were used as the corresponding climate indicators. The correlations between the temperature anomalies and the climate indices indicate that the tropospheric temperature variability in the mid-latitude (30-60N) linked to both AO and ENSO has been more pronounced over ocean than over land. However, the low stratospheric temperature variability in the mid-latitude is mainly associated with ENSO and QBO. The north-south symmetric patterns over the globe are seen in the wind anomaly distributions for ENSO and QBO, but not for AO. The ENSO events are globally vigorous but also localized during the recent 9 years compared with those based on the period of 1979-2011. The tropospheric warming and stratospheric cooling phenomena during this period are more remarkable in the recent 9 years, although according to IPCC (2012). their linkage to the ENSO variability is still uncertain. The ENSO is found to have more significant impact on the tropospheric and low stratosphere temperature variability over the tropics in the recent period, consistent with more active zonal wind meridional circulations. The discrepancies between satellite observations and MERRA are also discussed. The estimated relative impact of the three major concurrent large-scale climate phenomena on regional temperature variability can be of great use in its long-term predictability. (C) 2013 Elsevier Ltd. All rights reserved.
C1 [Yoo, Jung-Moon; Lee, Yu-Ri] Ewha Womans Univ, Dept Sci Educ, Seoul 120750, South Korea.
[Won, Young-In] NASA GSFC, Wyle IS, Greenbelt, MD 20771 USA.
[Jeong, Myeong-Jae] Gangneung Wonju Natl Univ, Dept Atmospher & Environm Sci, Gangwondo 210702, South Korea.
[Kim, Kyu-Myong] Morgan State Univ, Baltimore, MD 21251 USA.
[Shin, Dong-Bin; Lee, Yu-Ri; Cho, Young-Jun] Yonsei Univ, Dept Atmospher Sci, Seoul 120749, South Korea.
RP Yoo, JM (reprint author), Ewha Womans Univ, Dept Sci Educ, Seoul 120750, South Korea.
EM yjm@ewha.ac.kr
RI Kim, Kyu-Myong/G-5398-2014
FU National Research Foundation of Korea (NRF); Korea government (MEST)
[20120000858]; Korean Ministry of Environment
FX This work was supported by the National Research Foundation of Korea
(NRF) grant funded by Korea government (MEST) (No. 20120000858) and the
Korean Ministry of Environment as part of the Eco-Innovation Project. We
would like to thank Goddard Earth Sciences Data Information and Services
Center (GES DISC) for providing the AIRS/AMSU and MERRA data. We are
also grateful to NASA Land Process Distributed Active Archive Center (LP
DAAC) for providing the MODIS LST data.
NR 66
TC 2
Z9 2
U1 2
U2 9
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 1364-6826
J9 J ATMOS SOL-TERR PHY
JI J. Atmos. Sol.-Terr. Phys.
PD APR
PY 2013
VL 95-96
BP 15
EP 27
DI 10.1016/j.jastp.2013.01.002
PG 13
WC Geochemistry & Geophysics; Meteorology & Atmospheric Sciences
SC Geochemistry & Geophysics; Meteorology & Atmospheric Sciences
GA 122OB
UT WOS:000317326300002
ER
PT J
AU Choi, CJ
Seo, M
Choi, WS
Kim, KS
Youn, SA
Lindsey, T
Choi, YJ
Kim, CM
AF Choi, Chang-Jin
Seo, Min
Choi, Whan-Seok
Kim, Kyung-Soo
Youn, Sang-Ah
Lindsey, Tony
Choi, Yun-Jung
Kim, Churl-Min
TI Relationship Between Serum 25-Hydroxyvitamin D and Lung Function Among
Korean Adults in Korea National Health and Nutrition Examination Survey
(KNHANES), 2008-2010
SO JOURNAL OF CLINICAL ENDOCRINOLOGY & METABOLISM
LA English
DT Article
ID VITAMIN-D DEFICIENCY; RISK-FACTOR; DISEASE; TUBERCULOSIS; ASSOCIATION;
SUPPLEMENTATION; METAANALYSIS; INFECTIONS; PREVENTION; GUIDELINE
AB Context: The relationship between vitamin D status and pulmonary function has not been investigated for an East Asian population.
Objective: The aim of the present study was to examine the relationship of serum 25-hydroxyvitamin D [25(OH)D] with lung function in Korean adults.
Design and Setting: The analysis used data from the Korea National Health and Nutrition Examination Survey (KNHANES), a cross-sectional survey of Korean civilians, conducted from 2008 to 2010.
Participants: A total of 10 096 people aged 19 years and older were selected from 16 administrative districts in South Korea.
Main Outcome Measures: Serum 25(OH) D levels with lung function [forced expiratory volume in 1 second (FEV1) and forced vital capacity (FVC)].
Results: Serum 25(OH) D concentration was positively associated with lung function after controlling for age, sex, height, and season. For FEV1 and FVC, the differences between top and bottom quartiles in 25(OH) D were 51 mL (SE, 17 mL, P trend <.001) and 58 mL (SE, 20 mL, P trend <.005) greater volume, respectively. Association of serum 25(OH) D with FEV1 and FVC was only slightly attenuated after adjustment for body mass index, lifestyle and socioeconomic factors, and respiratory illness. The subjects with a history of pulmonary tuberculosis showed a much higher increase in FEV1; the difference between top and bottom quartiles in 25(OH) D was 229 mL (SE, 87 mL, P trend <.01).
Conclusion: Serum 25(OH) D levels have a positive correlation with pulmonary function. This relationship appears prominent in subjects with susceptibility to pulmonary tuberculosis. (J Clin Endocrinol Metab 98: 1703-1710, 2013)
C1 [Choi, Chang-Jin; Choi, Whan-Seok; Kim, Kyung-Soo; Youn, Sang-Ah; Kim, Churl-Min] Catholic Univ Korea, Dept Family Med, Seoul St Marys Hosp, Coll Med, Seoul 137701, South Korea.
[Seo, Min] Dankook Univ, Coll Med, Dept Parasitol, Cheonan 330715, South Korea.
[Lindsey, Tony] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Choi, Yun-Jung] Metabolex Inc, Hayward, CA 94545 USA.
RP Kim, CM (reprint author), Catholic Univ Korea, Dept Family Med, Seoul St Marys Hosp, Coll Med, 222 Banpo Daero, Seoul 137701, South Korea.
EM musofm@catholic.ac.kr
NR 32
TC 17
Z9 18
U1 0
U2 4
PU ENDOCRINE SOC
PI CHEVY CHASE
PA 8401 CONNECTICUT AVE, SUITE 900, CHEVY CHASE, MD 20815-5817 USA
SN 0021-972X
J9 J CLIN ENDOCR METAB
JI J. Clin. Endocrinol. Metab.
PD APR
PY 2013
VL 98
IS 4
BP 1703
EP 1710
DI 10.1210/jc.2012-3901
PG 8
WC Endocrinology & Metabolism
SC Endocrinology & Metabolism
GA 120TJ
UT WOS:000317195600076
PM 23533242
ER
PT J
AU Mallick, K
Jarvis, A
Fisher, JB
Tu, KP
Boegh, E
Niyogi, D
AF Mallick, Kaniska
Jarvis, Andrew
Fisher, Joshua B.
Tu, Kevin P.
Boegh, Eva
Niyogi, Dev
TI Latent Heat Flux and Canopy Conductance Based on Penman-Monteith,
Priestley-Taylor Equation, and Bouchet's Complementary Hypothesis
SO JOURNAL OF HYDROMETEOROLOGY
LA English
DT Article
ID RADIOMETRIC SURFACE-TEMPERATURE; CONVECTIVE BOUNDARY-LAYER;
ENERGY-BALANCE CLOSURE; CARBON-DIOXIDE; SENSIBLE HEAT; WATER-VAPOR;
REGIONAL EVAPOTRANSPIRATION; STOMATAL CONDUCTANCE; BIOSPHERE MODEL; PAN
EVAPORATION
AB A novel method is presented to analytically resolve the terrestrial latent heat flux (lambda E) and conductances (boundary layer g(B) and surface g(S)) using net radiation (R-N), ground heat flux (G), air temperature (T-a), and relative humidity (RH). This method consists of set of equations where the two unknown internal state variables (g(B) and g(S)) were expressed in terms of the known core variables, combining diffusion equations, the Penman-Monteith equation, the Priestley-Taylor equation, and Bouchet's complementary hypothesis. Estimated lambda E is validated with the independent eddy covariance lambda E observations over Soil Moisture Experiment 2002 (SMEX-02); the Global Energy and Water Cycle Experiment (GEWEX) Continental-Scale International Project (GCIP) selected sites from FLUXNET and tropics eddy flux, representing four climate zones (tropics, subtropics, temperate, and cold); and multiple biomes. The authors find a RMSE of 23.8-54.6 W m(-2) for hourly lambda E over SMEX-02 and GCIP and 23.8-29.0 W m(-2) for monthly lambda E over the FLUXNET and tropics. Observational and modeled evidence in the reduction in annual evaporation (E) pattern on the order of 33% from 1999 to 2006 was found in central Amazonia. Retrieved g(S) responded to vapor pressure deficit, measured lambda E, and gross photosynthesis in a theoretically robust behavior. However, the current scheme [Penman-Monteith-Bouchet-Lhomme (PMBL)] showed some overestimation of lambda E in limited soil moisture regimes. PMBL provides similar results when compared with another Priestley-Taylor-based lambda E estimation approach [Priestley-Taylor-Jet Propulsion Laboratory (PT-JPL)] but with the advantage of having the conductances analytically recovered.
C1 [Mallick, Kaniska; Fisher, Joshua B.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Jarvis, Andrew] Univ Lancaster, Lancaster Environm Ctr, Lancaster, England.
[Tu, Kevin P.] Pioneer HiBred Int Inc, Woodland, CA USA.
[Boegh, Eva] Roskilde Univ, Dept Environm Social & Spatial Change, Roskilde, Denmark.
[Niyogi, Dev] Purdue Univ, Dept Agron, W Lafayette, IN 47907 USA.
[Niyogi, Dev] Purdue Univ, Dept Earth & Atmospher & Planetary Sci, W Lafayette, IN 47907 USA.
RP Mallick, K (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM kaniska.mallick@gmail.com
OI Fisher, Joshua/0000-0003-4734-9085
FU Jet Propulsion Laboratory's Research and Technology Development Climate
Strategic Initiative; Natural Environment Research Council, United
Kingdom [NEE0191531]
FX We gratefully acknowledge NSIDC and CEOP for making the SMEX-02 and GCIP
data available. K. M. acknowledges the comments from Dr. Bill Kustas,
HRSL, USDA, and Dr. B. K. Bhattacharya, Space Applications Centre,
India. We also acknowledge the site PIs of the tropical forest eddy
covariance network and FLUXNET network for the data permission. We
acknowledge Dr. John Prueger for permitting us to use the SMEX-02. K. M.
also acknowledges Dr. Junhak Lee for his help in map preparation and the
postdoctoral research fellowship from the Jet Propulsion Laboratory's
Research and Technology Development Climate Strategic Initiative. D.N.
benefited in part through NSF CAREER (AGS-0847472, Anjuli Bamzai), USDA
NIFA 2011-68002-30220, and NSF INTEROP OCI 0753116. KM was partly funded
by the Natural Environment Research Council, United Kingdom, Grant
NEE0191531. Three anonymous reviewers are also acknowledged for their
helpful comments. The research was carried out at the Jet Propulsion
Laboratory, California Institute of Technology, under a contract with
the National Aeronautics and Space Administration.
NR 76
TC 11
Z9 11
U1 1
U2 39
PU AMER METEOROLOGICAL SOC
PI BOSTON
PA 45 BEACON ST, BOSTON, MA 02108-3693 USA
SN 1525-755X
EI 1525-7541
J9 J HYDROMETEOROL
JI J. Hydrometeorol.
PD APR
PY 2013
VL 14
IS 2
BP 419
EP 442
DI 10.1175/JHM-D-12-0117.1
PG 24
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 125SI
UT WOS:000317561200003
ER
PT J
AU Kirstetter, PE
Hong, Y
Gourley, JJ
Schwaller, M
Petersen, W
Zhang, J
AF Kirstetter, Pierre-Emmanuel
Hong, Y.
Gourley, J. J.
Schwaller, M.
Petersen, W.
Zhang, J.
TI Comparison of TRMM 2A25 Products, Version 6 and Version 7, with
NOAA/NSSL Ground Radar-Based National Mosaic QPE
SO JOURNAL OF HYDROMETEOROLOGY
LA English
DT Article
ID SURFACE REFERENCE TECHNIQUE; RAIN-PROFILING ALGORITHM; PRECIPITATION
RADAR; SATELLITE; VALIDATION
AB Characterization of the error associated with satellite rainfall estimates is a necessary component of deterministic and probabilistic frameworks involving spaceborne passive and active microwave measurements for applications ranging from water budget studies to forecasting natural hazards related to extreme rainfall events. The authors focus here on the relative error structure of Tropical Rainfall Measurement Mission (TRMM) precipitation radar (PR) quantitative precipitation estimation (QPE) at the ground by comparison of 2A25 products with reference values derived from NOAA/NSSL's ground radar-based National Mosaic and QPE system (NMQ/Q2). The primary contribution of this study is to compare the new 2A25, version 7 (V7), products that were recently released as a replacement of version 6 (V6). Moreover, the authors supply uncertainty estimates of the rainfall products so that they may be used in a quantitative manner for applications like hydrologic modeling. This new version is considered superior over land areas and will likely be the final version for TRMM PR rainfall estimates. Several aspects of the two versions are compared and quantified, including rainfall rate distributions, systematic biases, and random errors. All analyses indicate that V7 is in closer agreement with the reference rainfall compared to V6.
C1 [Kirstetter, Pierre-Emmanuel; Hong, Y.] Univ Oklahoma, Sch Civil Engn & Environm Sci, Norman, OK 73019 USA.
[Kirstetter, Pierre-Emmanuel; Gourley, J. J.; Zhang, J.] NOAA, Natl Severe Storms Lab, Norman, OK 73069 USA.
[Kirstetter, Pierre-Emmanuel; Hong, Y.] Natl Weather Ctr, Atmospher Radar Res Ctr, Norman, OK 73072 USA.
[Schwaller, M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Petersen, W.] NASA, Wallops Flight Facil, Wallops Isl, VA USA.
RP Hong, Y (reprint author), Natl Weather Ctr, Atmospher Radar Res Ctr, 120 David L Boren Blvd,Suite 4610, Norman, OK 73072 USA.
EM yanghong@ou.edu
RI Kirstetter, Pierre/E-2305-2013; Hong, Yang/D-5132-2009; Gourley,
Jonathan/C-7929-2016; Measurement, Global/C-4698-2015
OI Kirstetter, Pierre/0000-0002-7381-0229; Hong, Yang/0000-0001-8720-242X;
Gourley, Jonathan/0000-0001-7363-3755;
FU NASA Global Precipitation Measurement mission Ground Validation
Management
FX We are very much indebted to the team responsible for the NMQ/Q2
products, especially Carrie Langston. We want to thank two anonymous
reviewers, whose comments were very useful in improving the manuscript.
This work was funded by a postdoctoral grant from the NASA Global
Precipitation Measurement mission Ground Validation Management.
NR 34
TC 30
Z9 32
U1 0
U2 16
PU AMER METEOROLOGICAL SOC
PI BOSTON
PA 45 BEACON ST, BOSTON, MA 02108-3693 USA
SN 1525-755X
EI 1525-7541
J9 J HYDROMETEOROL
JI J. Hydrometeorol.
PD APR
PY 2013
VL 14
IS 2
BP 661
EP 669
DI 10.1175/JHM-D-12-030.1
PG 9
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 125SI
UT WOS:000317561200017
ER
PT J
AU Sanghavi, S
Natraj, V
AF Sanghavi, Suniti
Natraj, Vijay
TI Using analytic derivatives to assess the impact of phase function
Fourier decomposition technique on the accuracy of a radiative transfer
model
SO JOURNAL OF QUANTITATIVE SPECTROSCOPY & RADIATIVE TRANSFER
LA English
DT Article
DE Fourier decomposition; Legendre expansion; Aerosol phase function;
Interpolation error; Jacobian matrix
ID DISCRETE SPACE THEORY; POLARIZED-LIGHT; SCATTERING; RELEVANT; MATRIX
AB Fourier decomposition of the phase function is essential to decouple the azimuthal component of the radiative transfer equation for multiple scattering calculations. This decomposition can be carried out by means of a direct numerical method based on the definition of the Fourier transform (numFT), or by an expansion of the phase function in terms of spherical Legendre polynomials (sphFT). numFT requires interpolation of the phase function between discrete angles, leading to spurious errors in the final computations. This error is difficult to quantify by means of intensity-only computations, since it is hard to determine the absolute accuracy of any given approach. We show that a linearization (analytic computation of derivatives) of the intensity with respect to parameters governing the phase function can be compared against results using the finite difference method, thereby providing a self-consistency test for characterizing and quantifying the error.
We have applied this approach to two linearized versions of the Matrix Operator Method, which are identical in all respects except that one uses numFT while the other uses sphFT. In both cases, we compute the derivatives of the intensity with respect to aerosol 'parameters governing scattering in the simulated atmosphere. Comparison of the derivatives against their finite difference estimates shows a reduction of error by several orders of magnitude when Legendre polynomials are employed. We have also examined the effect of the angular resolution of the phase function on the error due to the numFT technique. A general reduction of error is seen with increasing angular resolution, indicating that interpolation is indeed the major error source. Also, we have pointed out a related source of error in numFT computations that occurs when Fourier decomposition is carried out on the composite phase function of a layer consisting of more than one scatterer. We conclude that an expansion of the phase function in terms of Legendre polynomials eliminates the need for interpolation, making it the more suitable method for linearization of radiative transfer, especially with respect to aerosol properties. (C) 2013 Elsevier Ltd. All rights reserved.
C1 [Sanghavi, Suniti; Natraj, Vijay] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Sanghavi, S (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM suniti.sanghavi@gmail.com
NR 18
TC 2
Z9 2
U1 1
U2 3
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0022-4073
J9 J QUANT SPECTROSC RA
JI J. Quant. Spectrosc. Radiat. Transf.
PD APR
PY 2013
VL 119
BP 137
EP 149
DI 10.1016/j.jqsrt.2012.12.028
PG 13
WC Optics; Spectroscopy
SC Optics; Spectroscopy
GA 126QK
UT WOS:000317636100013
ER
PT J
AU Marchi, S
Bottke, WF
Cohen, BA
Wunnemann, K
Kring, DA
McSween, HY
De Sanctis, MC
O'Brien, DP
Schenk, P
Raymond, CA
Russell, CT
AF Marchi, S.
Bottke, W. F.
Cohen, B. A.
Wuennemann, K.
Kring, D. A.
McSween, H. Y.
De Sanctis, M. C.
O'Brien, D. P.
Schenk, P.
Raymond, C. A.
Russell, C. T.
TI High-velocity collisions from the lunar cataclysm recorded in asteroidal
meteorites
SO NATURE GEOSCIENCE
LA English
DT Article
ID LATE HEAVY BOMBARDMENT; INNER SOLAR-SYSTEM; PARENT BODY; IMPACT;
CONSTRAINTS; HISTORY; VESTA; AGES; CRATER; BELT
AB The Moon experienced an intense period of impacts about 4 Gyr ago. This cataclysm is thought to have affected the entire inner Solar System and has been constrained by the radiometric dating of lunar samples: Ar-40-Ar-39 ages reflect the heating and degassing of target rocks by large basin-forming impacts on the Moon. Radiometric dating of meteorites from Vesta and the H-chondrite parent body also shows numerous Ar-40-Ar-39 ages between 3.4 and 4.1 Gyr ago, despite a different dynamical context, where impacts typically occur at velocities too low to reset geochronometers. Here we interpret the Ar-40-Ar-39 age record in meteorites to reflect unusually high impact velocities exceeding 10 km s(-1). Compared with typical impact velocities for main-belt asteroids of about 5 km s(-1), these collisions would produce 100-1,000 times more highly heated material by volume. We propose that the Ar-40-Ar-39 ages between 3.4 and 4.1 Gyr ago from Vesta, the H-chondrite parent body and the Moon record impacts from numerous main-belt asteroids that were driven onto high-velocity and highly eccentric orbits by the effects of the late migration of the giant planets. We suggest that the bombardment persisted for many hundreds of millions of years and affected most inner Solar System bodies.
C1 [Marchi, S.; Bottke, W. F.] NASA Lunar Sci Inst, SW Res Inst, Boulder, CO 80302 USA.
[Cohen, B. A.] NASA Marshall Space Flight Ctr, Huntsville, AL 35805 USA.
[Wuennemann, K.] Museum Nat Kunde, D-10115 Berlin, Germany.
[Kring, D. A.] NASA Lunar Sci Inst, USRA Lunar & Planetary Inst, Houston, TX 77058 USA.
[McSween, H. Y.] Univ Tennessee, Knoxville, TN 37996 USA.
[De Sanctis, M. C.] Ist Nazl Astrofis, I-00133 Rome, Italy.
[O'Brien, D. P.] Planetary Sci Inst, Tucson, AZ 85719 USA.
[Schenk, P.] Lunar & Planetary Inst, Houston, TX 77058 USA.
[Raymond, C. A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Russell, C. T.] Univ Calif Los Angeles, Los Angeles, CA 90024 USA.
RP Marchi, S (reprint author), NASA Lunar Sci Inst, SW Res Inst, Boulder, CO 80302 USA.
EM marchi@boulder.swri.edu
RI De Sanctis, Maria Cristina/G-5232-2013
OI De Sanctis, Maria Cristina/0000-0002-3463-4437
FU NASA Lunar Science Institute (Center for Lunar Origin and Evolution at
the Southwest Research Institute in Boulder, Colorado- NASA)
[NNA09DB32A]; NASA Lunar Science Institute (Center for Lunar Science and
Exploration at the Lunar and Planetary Institute in Houston, Texas);
Helmholtz-Alliance 'Planetary Evolution and Life'; Agenzia Spaziale
Italiana; NASA High-End Computing (HEC) Program through the NASA
Advanced Supercomputing (NAS) Division at Ames Research Center
FX We thank D. Bogard, B. Ivanov, A. Morbidelli, D. Nesvorny, T. Swindle
and the Dawn Science Team for helpful discussions and insightful
comments. The contributions of S. M., W. F. B., B. A. C. and D. A. K.
were supported by the NASA Lunar Science Institute (Center for Lunar
Origin and Evolution at the Southwest Research Institute in Boulder,
Colorado- NASA Grant NNA09DB32A; Center for Lunar Science and
Exploration at the Lunar and Planetary Institute in Houston, Texas). The
contribution of K. W. was funded by the Helmholtz-Alliance 'Planetary
Evolution and Life'. D.P.O'B. and P. S. thank the NASA Dawn at Vesta
Participating Scientist Program. The contribution of M. C. D. S. was
partially supported by Agenzia Spaziale Italiana. Resources supporting
this work were provided by the NASA High-End Computing (HEC) Program
through the NASA Advanced Supercomputing (NAS) Division at Ames Research
Center.
NR 47
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U1 2
U2 30
PU NATURE PUBLISHING GROUP
PI NEW YORK
PA 75 VARICK ST, 9TH FLR, NEW YORK, NY 10013-1917 USA
SN 1752-0894
J9 NAT GEOSCI
JI Nat. Geosci.
PD APR
PY 2013
VL 6
IS 4
BP 303
EP 307
DI 10.1038/NGEO1769
PG 5
WC Geosciences, Multidisciplinary
SC Geology
GA 117IJ
UT WOS:000316946500020
ER
PT J
AU Larsson, R
McKay, CP
AF Larsson, Richard
McKay, Christopher P.
TI Timescale for oceans in the past of Titan
SO PLANETARY AND SPACE SCIENCE
LA English
DT Article
DE Titan; Surface; Methane ocean; Planetary evolution
ID ATMOSPHERE; LAKES; CYCLE
AB We estimate the past extent of liquid on the surface of Titan as a function of time assuming the current rate of destruction of methane and no sources or subsurface sinks. As methane increases for increasing past time the polar lakes expand equatorward. We use a spherical harmonics model for the surface topography to compute the fraction of the surface covered as the methane inventory increases. We find that substantial parts of the equator would have been flooded by a polar ocean 300 million years ago and that the equator would have been connected to a global ocean 600 million years ago. This provides one possible explanation for the fluvial features seen at the equator on Titan. (C) 2012 Elsevier Ltd. All rights reserved.
C1 [Larsson, Richard] Lulea Univ Technol, Dept Comp Sci Elect & Space Engn, SE-98128 Kiruna, Sweden.
[McKay, Christopher P.] NASA, Ames Res Ctr, Div Space Sci & Astrobiol, Moffett Field, CA 94035 USA.
RP Larsson, R (reprint author), Lulea Univ Technol, Dept Comp Sci Elect & Space Engn, Space Campus 1, SE-98128 Kiruna, Sweden.
EM ric.larsson@gmail.com
OI Larsson, Richard/0000-0001-6719-723X
NR 29
TC 6
Z9 6
U1 0
U2 9
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0032-0633
J9 PLANET SPACE SCI
JI Planet Space Sci.
PD APR
PY 2013
VL 78
BP 22
EP 24
DI 10.1016/j.pss.2012.12.001
PG 3
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 128YX
UT WOS:000317806700002
ER
PT J
AU Scott, JM
Koelwyn, GJ
Hornsby, WE
Khouri, M
Peppercorn, J
Douglas, PS
Jones, LW
AF Scott, Jessica M.
Koelwyn, Graeme J.
Hornsby, Whitney E.
Khouri, Michel
Peppercorn, Jeffrey
Douglas, Pamela S.
Jones, Lee W.
TI Exercise Therapy as Treatment for Cardiovascular and Oncologic Disease
After a Diagnosis of Early-Stage Cancer
SO SEMINARS IN ONCOLOGY
LA English
DT Review
ID ANDROGEN DEPRIVATION THERAPY; RANDOMIZED CONTROLLED-TRIAL; C-REACTIVE
PROTEIN; ADVANCED PROSTATE-CANCER; EARLY BREAST-CANCER; CELL
LUNG-CANCER; PHYSICAL-ACTIVITY; POSTMENOPAUSAL WOMEN; OXIDATIVE STRESS;
METABOLIC SYNDROME
C1 [Scott, Jessica M.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA.
[Scott, Jessica M.] Univ Space Res Assoc, Houston, TX USA.
[Koelwyn, Graeme J.] Univ British Columbia, Sch Hlth & Exercise Sci, Kelowna, BC, Canada.
[Hornsby, Whitney E.; Khouri, Michel; Peppercorn, Jeffrey; Douglas, Pamela S.; Jones, Lee W.] Duke Univ, Med Ctr, Durham, NC USA.
RP Jones, LW (reprint author), Duke Canc Inst, Box 3085, Durham, NC 27710 USA.
EM lee.w.jones@duke.edu
FU National Institutes of Health [CA143254, CA142566, CA138634, CA133895]
FX L.W.J. was supported by National Institutes of Health grants no.
CA143254, CA142566, CA138634, and CA133895 and with funds from George
and Susan Beischer. The other authors report no potential conflicts of
interest.
NR 118
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U1 2
U2 11
PU W B SAUNDERS CO-ELSEVIER INC
PI PHILADELPHIA
PA 1600 JOHN F KENNEDY BOULEVARD, STE 1800, PHILADELPHIA, PA 19103-2899 USA
SN 0093-7754
J9 SEMIN ONCOL
JI Semin. Oncol.
PD APR
PY 2013
VL 40
IS 2
BP 218
EP 228
DI 10.1053/j.seminoncol.2013.01.001
PG 11
WC Oncology
SC Oncology
GA 129VA
UT WOS:000317870900010
PM 23540747
ER
PT J
AU Wiens, RC
Maurice, S
Lasue, J
Forni, O
Anderson, RB
Clegg, S
Bender, S
Blaney, D
Barraclough, BL
Cousin, A
Deflores, L
Delapp, D
Dyar, MD
Fabre, C
Gasnault, O
Lanza, N
Mazoyer, J
Melikechi, N
Meslin, PY
Newsom, H
Ollila, A
Perez, R
Tokar, RL
Vaniman, D
AF Wiens, R. C.
Maurice, S.
Lasue, J.
Forni, O.
Anderson, R. B.
Clegg, S.
Bender, S.
Blaney, D.
Barraclough, B. L.
Cousin, A.
Deflores, L.
Delapp, D.
Dyar, M. D.
Fabre, C.
Gasnault, O.
Lanza, N.
Mazoyer, J.
Melikechi, N.
Meslin, P. -Y.
Newsom, H.
Ollila, A.
Perez, R.
Tokar, R. L.
Vaniman, D.
TI Pre-flight calibration and initial data processing for the Chem Cam
laser-induced breakdown spectroscopy instrument on the Mars Science
Laboratory rover
SO SPECTROCHIMICA ACTA PART B-ATOMIC SPECTROSCOPY
LA English
DT Article
DE Laser-induced breakdown spectroscopy; LIBS; Mars; Curiosity rover;
ChemCam
ID PLIOCENE MACUSANI VOLCANICS; SE PERU; PLASMA; SULFUR; EXPLORATION;
ATMOSPHERE; MINERALOGY; CHEMISTRY; EMISSION; OUTCROPS
AB The ChemCam instrument package on the Mars Science Laboratory rover, Curiosity, is the first planetary science instrument to employ laser-induced breakdown spectroscopy (LIBS) to determine the compositions of geological samples on another planet. Pre-processing of the spectra involves subtracting the ambient light background, removing noise, removing the electron continuum, calibrating for the wavelength, correcting for the variable distance to the target, and applying a wavelength-dependent correction for the instrument response. Further processing of the data uses multivariate and univariate comparisons with a LIBS spectral library developed prior to launch as well as comparisons with several on-board standards post-landing. The level-2 data products include semi-quantitative abundances derived from partial least squares regression.
A LIBS spectral library was developed using 69 rock standards in the form of pressed powder disks, glasses, and ceramics to minimize heterogeneity on the scale of the observation (350-550 mu m dia.). The standards covered typical compositional ranges of igneous materials and also included sulfates, carbonates, and phyllosilicates. The provenance and elemental and mineralogical compositions of these standards are described. Spectral characteristics of this data set are presented, including the size distribution and integrated irradiances of the plasmas, and a proxy for plasma temperature as a function of distance from the instrument. Two laboratory-based clones of ChemCam reside in Los Alamos and Toulouse for the purpose of adding new spectra to the database as the need arises. Sensitivity to differences in wavelength correlation to spectral channels and spectral resolution has been investigated, indicating that spectral registration needs to be within half a pixel and resolution needs to match within 1.5 to 2.6 pixels. Absolute errors are tabulated for derived compositions of each major element in each standard using PLS regression. Sources of errors are investigated and discussed, and methods for improving the analytical accuracy of compositions derived from ChemCam spectra are discussed. Published by Elsevier B.V.
C1 [Wiens, R. C.; Clegg, S.; Cousin, A.; Delapp, D.; Lanza, N.] Los Alamos Natl Lab, Los Alamos, NM 87544 USA.
[Maurice, S.; Lasue, J.; Forni, O.; Cousin, A.; Gasnault, O.; Meslin, P. -Y.] Inst Rech Astrophys & Planetol, Toulouse, France.
[Anderson, R. B.] US Geol Survey, Flagstaff, AZ 86001 USA.
[Bender, S.; Barraclough, B. L.; Tokar, R. L.; Vaniman, D.] Planetary Sci Inst, Tucson, AZ USA.
[Blaney, D.; Deflores, L.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Dyar, M. D.] Mt Holyoke Coll, S Hadley, MA 01075 USA.
[Fabre, C.] Georessources, Nancy, France.
[Mazoyer, J.] Observ Paris, LESIA, Meudon, France.
[Melikechi, N.] Delaware State Univ, Dover, DE USA.
[Newsom, H.; Ollila, A.] Univ New Mexico, Albuquerque, NM 87131 USA.
[Perez, R.] Ctr Natl Etud Spatiale, Toulouse, France.
RP Wiens, RC (reprint author), Los Alamos Natl Lab, POB 1663, Los Alamos, NM 87544 USA.
EM rwiens@lanl.gov
RI Gasnault, Olivier/F-4327-2010;
OI Gasnault, Olivier/0000-0002-6979-9012; Forni,
Olivier/0000-0001-6772-9689; Clegg, Sam/0000-0002-0338-0948
FU NASA Mars Program Office for ChemCam; CNES
FX The ChemCam team is grateful for support from the NASA Mars Program
Office for ChemCam, and from CNES. We also gratefully acknowledge the
Los Alamos National Laboratory's laboratory-directed research and
development exploratory research (LDRD-ER) program for supporting early
MVA studies. Many people supported the ChemCam instrument that was used
to carry out these studies, and we are particularly grateful to other
ChemCam team members who supported this work B. Banisadr is thanked for
his contributions to the total emission studies.
NR 52
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U2 67
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0584-8547
J9 SPECTROCHIM ACTA B
JI Spectroc. Acta Pt. B-Atom. Spectr.
PD APR 1
PY 2013
VL 82
BP 1
EP 27
DI 10.1016/j.sab.2013.02.003
PG 27
WC Spectroscopy
SC Spectroscopy
GA 124DG
UT WOS:000317443400001
ER
PT J
AU Lock, JA
Ball, DW
AF Lock, James A.
Ball, David W.
TI Why Is the Sky Blue?
SO SPECTROSCOPY
LA English
DT Article
AB There are many ways in which spectroscopy is relevant to matters celestial. Here, we'll tackle one of the classic ones, one to which many know the simple explanation, but few know the details. In this column, we'll go over the details.
C1 [Lock, James A.; Ball, David W.] Cleveland State Univ, Cleveland, OH 44115 USA.
[Lock, James A.] NASA, Glenn Res Ctr, Cleveland, OH USA.
RP Lock, JA (reprint author), Cleveland State Univ, Cleveland, OH 44115 USA.
EM d.ball@csuohio.edu
NR 2
TC 0
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U1 2
U2 12
PU ADVANSTAR COMMUNICATIONS INC
PI DULUTH
PA 131 W 1ST STREET, DULUTH, MN 55802 USA
SN 0887-6703
J9 SPECTROSCOPY-US
JI Spectroscopy
PD APR
PY 2013
VL 28
IS 4
BP 12
EP 17
PG 6
WC Spectroscopy
SC Spectroscopy
GA 125RQ
UT WOS:000317559400003
ER
PT J
AU Griffith, P
Williamson, R
AF Griffith, Peter
Williamson, Ruth
TI Interview with Dr Peter Griffith
SO CARBON MANAGEMENT
LA English
DT Editorial Material
AB Dr Peter Griffith received his PhD in Ecology from the University of Georgia (GA, USA), his MSc in Marine, Estuarine and Environmental Science from the University of Maryland (MD, USA) and a BSc with Honors in Botany and Zoology from Duke University (NC, USA). Dr Griffith is now the founding director of the National Aeronautics and Space Administration (NASA) Carbon Cycle and Ecosystems Office, supporting the North American Carbon Program, a component of the US Global Change Research Program designed to quantify continental-scale carbon sources and sinks in North America, NASA's Arctic Boreal Vulnerability Experiment, and the NASA Carbon Cycle and Ecosystems Focus Area. As a distinguished expert in carbon cycles, Dr Griffith speaks to Ruth Williamson, Commissioning Editor of Carbon Management, about the changes in carbon cycle research throughout his career, important advances in our understanding of climate science, and important obstacles and future directions for carbon cycle scientists.
C1 [Griffith, Peter] NASA, Goddard Space Flight Ctr, Sigma Space Corp, Greenbelt, MD 20771 USA.
RP Griffith, P (reprint author), NASA, Goddard Space Flight Ctr, Sigma Space Corp, Code 618, Greenbelt, MD 20771 USA.
RI Griffith, Peter/I-1392-2016
OI Griffith, Peter/0000-0002-4267-7429
NR 7
TC 0
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U1 0
U2 0
PU FUTURE SCI LTD
PI LONDON
PA UNITED HOUSE, 2 ALBERT PL, LONDON, N3 1QB, ENGLAND
SN 1758-3004
J9 CARBON MANAG
JI Carbon Manag.
PD APR
PY 2013
VL 4
IS 2
BP 119
EP 123
DI 10.4155/CMT.13.7
PG 5
WC Environmental Sciences; Environmental Studies
SC Environmental Sciences & Ecology
GA 114XT
UT WOS:000316777000008
ER
PT J
AU Walker, RT
Bergman, EA
Elliott, JR
Fielding, EJ
Ghods, AR
Ghoraishi, M
Jackson, J
Nazari, H
Nemati, M
Oveisi, B
Talebian, M
Walters, RJ
AF Walker, R. T.
Bergman, E. A.
Elliott, J. R.
Fielding, E. J.
Ghods, A. -R.
Ghoraishi, M.
Jackson, J.
Nazari, H.
Nemati, M.
Oveisi, B.
Talebian, M.
Walters, R. J.
TI The 2010-2011 South Rigan (Baluchestan) earthquake sequence and its
implications for distributed deformation and earthquake hazard in
southeast Iran
SO GEOPHYSICAL JOURNAL INTERNATIONAL
LA English
DT Article
DE Radar interferometry; Seismicity and tectonics; Body waves; Continental
neotectonics; Asia
ID DASHT-E-BAYAZ; EASTERN IRAN; FAULT SLIP; SURFACE DEFORMATION; ACTIVE
TECTONICS; GPS MEASUREMENTS; SATELLITE RADAR; MIDDLE-EAST; INSAR;
RELOCATION
AB We investigate the source processes and tectonic significance of two earthquakes that occurred on 2010 December 20 (M-w 6.5) and 2011 January 27 (M-w 6.2) within a desert region south of the town of Rigan, SE Iran. The two earthquakes, which we refer to as the South Rigan events, occurred close to one another at the northern margin of the Shahsavaran mountains: a mainly volcanic chain in which the potential for active faulting has not previously been considered in detail. Surface displacements mapped using SAR interferometry, multiple-event relocation analysis of epicentres, body-waveform modelling and field measurements of surface rupture together reveal that the 2010 December 20 earthquake involved an average of similar to 1.3 m right-lateral slip on a vertical fault trending similar to 210 degrees whereas the 2011 January 27 resulted from similar to 0.6 m of slip on a conjugate left-lateral fault striking similar to 310 degrees, parallel to the trend of the Shahsavaran mountains and confined within a zone of increased Coulomb stress from the earlier main shock. The main slip for the 2010 and 2011 main shocks failed to reach the surface though minor cracks and en-echelon fissures were mapped following both events. Some of the surface cracks may have been enhanced during a period of minor afterslip in the days following the 2010 main shock. Using the insights gained from our investigation of the two South Rigan earthquakes we perform a regional reconnaissance of the active faulting using SPOTS (2.5 m) satellite imagery. We show that distributed similar to N-S right-lateral faulting is widely distributed north of the Shahsavaran mountains. We also show evidence for left-lateral strike-slip faulting parallel to the Shahsavaran mountains, with a component of extension in the east and shortening in the west, which is likely to accommodate regional N-S right-lateral shearing by clockwise rotation about a vertical axis. The distributed strike-slip faulting is closely associated with the distribution of towns and villages and constitutes a continuing hazard to local populations.
C1 [Walker, R. T.; Elliott, J. R.; Walters, R. J.] Univ Oxford, Dept Earth Sci, Oxford OX1 3AN, England.
[Bergman, E. A.] Univ Colorado, Dept Phys, Ctr Imaging Earths Interior, Boulder, CO 80309 USA.
[Fielding, E. J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Ghods, A. -R.] IASBS, Dept Earth Sci, Zanjan, Iran.
[Ghoraishi, M.; Nazari, H.; Talebian, M.] Geol Survey Iran, Res Inst Earth Sci, Tehran, Iran.
[Jackson, J.] Univ Cambridge, Bullard Labs, Cambridge CB1 3EZ, England.
[Nemati, M.] Bahonar Univ Kerman, Fac Sci, Dept Geol, Kerman, Iran.
[Nemati, M.; Oveisi, B.] Geol Survey Iran, Seismotecton Dept, Tehran, Iran.
RP Walker, RT (reprint author), Univ Oxford, Dept Earth Sci, S Parks Rd, Oxford OX1 3AN, England.
EM Richard.Walker@earth.ox.ac.uk
RI Elliott, John/B-8200-2011; Walker, Richard/D-9908-2011; Walters,
Richard/G-7114-2012; Fielding, Eric/A-1288-2007
OI Elliott, John/0000-0003-2957-4596; Walters, Richard/0000-0002-1704-8727;
Fielding, Eric/0000-0002-6648-8067
FU Geological Survey of Iran; NASA Earth Surface and Interior Focus Area;
ESA [AOALO.3598]; AO PI project [LAN0190, 2214]; NERC; Royal Society of
London; OSUG (Observatoire des Sciences de l'Univers de Grenoble)
Visiting Fellowship
FX We thank the Geological Survey of Iran for their support of our work in
Iran and for enabling field visits to the epicentral region. We also
thank the IIEES (International Institute of Earthquake Engineering and
Seismology), IRSC (Iranian Seismological Centre), and BHRC (Building and
Housing research Centre) for access to instrumental records. Part of the
research described in this paper was supported by the NASA Earth Surface
and Interior Focus Area and performed at the Jet Propulsion Laboratory,
California Institute of Technology under contract with NASA. E K Nissen
helped with the initial body-waveform analysis. We thank Sylvain Barbot
and Manuel Berberian for detailed and constructive review comments.
SPOTS satellite imagery was provided by the European Space Agency
through project allocation No. C1P.6462. ALOS PALSAR data is copyright
JAXA, METI and was provided by ESA under project AOALO.3598. TerraSAR-X
data is copyright 2010, 2011 DLR and was provided under AO PI project
LAN0190. COSMO-SkyMed data is copyright 2010, 2011 ASI and was provided
under AO PI project 2214. We also thank the NERC-ESRC Earthquakes
without Frontiers (EwF) program and the NERC-funded NCEO/COMET+ centre
in the UK. RTW is supported by a University Research Fellowship from the
Royal Society of London and wrote the manuscript at Universite Joseph
Fourier in Grenoble, France, whereas supported by an OSUG (Observatoire
des Sciences de l'Univers de Grenoble) Visiting Fellowship.
NR 49
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U1 1
U2 22
PU OXFORD UNIV PRESS
PI OXFORD
PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND
SN 0956-540X
EI 1365-246X
J9 GEOPHYS J INT
JI Geophys. J. Int.
PD APR
PY 2013
VL 193
IS 1
BP 349
EP 374
DI 10.1093/gji/ggs109
PG 26
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 120KW
UT WOS:000317170200026
ER
PT J
AU Janches, D
Hormaechea, JL
Brunini, C
Hocking, W
Fritts, DC
AF Janches, D.
Hormaechea, J. L.
Brunini, C.
Hocking, W.
Fritts, D. C.
TI An initial meteoroid stream survey in the southern hemisphere using the
Southern Argentina Agile Meteor Radar (SAAMER)
SO ICARUS
LA English
DT Article
ID ORBIT-RADAR; METHODOLOGY; RADIANTS; ORIGIN; DISKS
AB We present in this manuscript a 4 year survey of meteor shower radiants utilizing the Southern Argentina Agile Meteor Radar (SAAMER). SAAMER, which operates at the southern most region of South America, is a new generation SKiYMET system designed with significant differences from typical meteor radars including high transmitted power and an 8-antenna transmitting array enabling large detected rates at low zenith angles. We applied the statistical methodology developed by Jones and Jones (Jones, J., Jones, W. [2006]. Month. Not. R. Astron. Soc. 367, 1050-1056) to the data collected each day and compiled the results into 1 composite representative year at 1 degrees resolution in Solar Longitude. We then search for enhancements in the activity which last for at least 3 days and evolve temporally as is expected from a meteor shower. Using this methodology, we have identified in our data 32 shower radiants, two of which were not part of the IAU commission 22 meteor shower working list. Recently, SAAMER's capabilities were enhanced by adding two remote stations to receive meteor forward scatter signals from meteor trails and thus enable the determination of meteoroid orbital parameters. SAAMER started recording orbits in January 2012 and future surveys will focus on the search for unknown meteor streams, in particular in the southern ecliptic sky. Published by Elsevier Inc.
C1 [Janches, D.] NASA, Goddard Space Flight Ctr, Space Weather Lab, Greenbelt, MD 20771 USA.
[Hormaechea, J. L.] Estn Astron Rio Grande, Rio Grande, Tierra del Fueg, Argentina.
[Brunini, C.] Univ Nacl La Plata, Dept Ciencias Astron & Geofis, La Plata, Buenos Aires, Argentina.
[Hocking, W.] Univ Western Ontario, Dept Phys & Astron, London, ON N6A 3K7, Canada.
[Fritts, D. C.] Gats Inc, Boulder, CO 80302 USA.
RP Janches, D (reprint author), NASA, Goddard Space Flight Ctr, Space Weather Lab, Mail Code 674, Greenbelt, MD 20771 USA.
EM diego.janches@nasa.gov; jlhor@earg.gov.ar; claudiobrunini@yahoo.com;
whocking@uwo.ca; dave@gats-inc.com
RI Janches, Diego/D-4674-2012;
OI Janches, Diego/0000-0001-8615-5166; Hormaechea, Jose
Luis/0000-0003-4533-3282
FU NSF [AGS - 0634650, AGS - 0944104, AST - 0908118]
FX This work was supported by NSF Awards AGS - 0634650, AGS - 0944104 and
AST - 0908118. We wish to thank the EARG personnel for their invaluable
help with the operation of SAAMER and D. Moser, P. Brown and M.
Campbell-Brown for useful discussions.
NR 24
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U1 0
U2 2
PU ACADEMIC PRESS INC ELSEVIER SCIENCE
PI SAN DIEGO
PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA
SN 0019-1035
EI 1090-2643
J9 ICARUS
JI Icarus
PD APR
PY 2013
VL 223
IS 2
BP 677
EP 683
DI 10.1016/j.icarus.2012.12.018
PG 7
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 116ZZ
UT WOS:000316923200004
ER
PT J
AU Tice, DS
Irwin, PGJ
Fletcher, LN
Teanby, NA
Hurley, J
Orton, GS
Davis, GR
AF Tice, Dane S.
Irwin, Patrick G. J.
Fletcher, Leigh N.
Teanby, Nick A.
Hurley, Jane
Orton, Glenn S.
Davis, Gary R.
TI Uranus' cloud particle properties and latitudinal methane variation from
IRTF SpeX observations
SO ICARUS
LA English
DT Article
DE Uranus, Atmosphere; Atmospheres, Composition; Atmospheres, Structure;
Data reduction techniques
ID INFRARED-ABSORPTION SPECTRA; OVERTONE BAND; TEMPERATURES; HYDROGEN; CH4;
SPECTROGRAPH; ATMOSPHERE; PLANETS; CM(-1); UKIRT
AB The Uranian atmosphere was observed in August 2009 from 0.8 to 1.8 mu m using the near-infrared spectrometer, SpeX, at NASA's Infrared Telescope Facility. The observations had a spectral resolution of R=1200 and an average seeing of between 0.5" in the H-Band (1.4-1.8 mu m) and 0.6" in the I-Band (0.8-0.9 mu m). The reduced data were analyzed with a multiple-scattering retrieval code. We were able to reproduce observations when using a vertically-compact cloud in the upper troposphere and a vertically-extended, optically-thin haze above the 1-bar level. The existence of these two clouds is consistent with previous studies.
The sub-micron portion of the data are most sensitive to very small scattering particles, allowing more insight into particle size than other portions of the infrared spectrum. This portion of the spectrum was therefore of particular interest and was not available in most previous studies of the planet. We assumed the particles in both clouds to be relatively strong forward scatterers (with a Henyey-Greenstein asymmetry factor of g = 0.7). Given this assumption, we found single-scattering albedos in the tropospheric cloud particles to be (omega) over bar = 0.7 at wavelengths above 1.4 mu m and to gradually increase to (omega) over bar = 1.0 at wavelengths shortward of 1.0 mu m. In the upper haze, we found single-scattering albedos to be (omega) over bar = 1.0 with the exception of a narrow drop at 1.0 mu m to (omega) over bar = 0.6. We found a preference for upper haze particle radii at r = 0.10 mu m. Retrievals of base pressure, fractional scale height, and optical depth in both cloud layers showed the best agreement with data when the base pressure of the upper haze was fixed just above the tropospheric clouds, rather than at or above the tropopausal cold trap. We found that these same retrievals strongly preferred tropospheric cloud particles of 1.35-mu m radii, and observed cloud top height to increase away from the equator in the case of latitudinally invariant methane abundance.
Latitudinal methane variability was also considered, both through a reflectivity study at the 825-nm collision-induced hydrogen absorption feature, as well as through radiative transfer analysis, using forward modeling and retrievals of cloud properties and methane abundance. The data suggested that methane abundance above the tropospheric clouds increased when moving from the midlatitudes towards the equator by at least 9%. The peak of this equatorial methane enrichment was determined to be at 4 +/- 2 degrees S latitude, having moved nearly 15 degrees northward since a reflectance study of 2002 data (Karkoschka and Tomasko, 2009). (C) 2013 Elsevier Inc. All rights reserved.
C1 [Tice, Dane S.; Irwin, Patrick G. J.; Fletcher, Leigh N.; Hurley, Jane] Univ Oxford, Dept Phys, Clarendon Lab, Oxford OX1 3PU, England.
[Teanby, Nick A.] Univ Bristol, Sch Earth Sci, Bristol BS8 1RJ, Avon, England.
[Orton, Glenn S.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Davis, Gary R.] Joint Astron Ctr, Hilo, HI 96720 USA.
RP Tice, DS (reprint author), Univ Oxford, Dept Phys, Clarendon Lab, Parks Rd, Oxford OX1 3PU, England.
EM tice@atm.ox.ac.uk
RI Fletcher, Leigh/D-6093-2011;
OI Fletcher, Leigh/0000-0001-5834-9588; Teanby,
Nicholas/0000-0003-3108-5775; Irwin, Patrick/0000-0002-6772-384X
FU United Kingdom Science and Technologies Facilities Council; University
of Oxford Glasstone Fellowship; Leverhulme Trust; NASA
FX We are grateful for project funding from the United Kingdom Science and
Technologies Facilities Council, the University of Oxford Glasstone
Fellowship (Fletcher), the Leverhulme Trust (Teanby), and a grant from
NASA to the Jet Propulsion Laboratory, California Institute of
Technology (Orton). We would like to thank our IRTF support astronomer,
Bobby Bus, and all the staff at the Infrared Telescope Facility. IRTF is
operated by the University of Hawaii under Cooperative Agreement No.
NNX-08AE38A with the National Aeronautics and Space Administration,
Science Mission Directorate, Planetary Astronomy Program.
NR 30
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U1 0
U2 7
PU ACADEMIC PRESS INC ELSEVIER SCIENCE
PI SAN DIEGO
PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA
SN 0019-1035
J9 ICARUS
JI Icarus
PD APR
PY 2013
VL 223
IS 2
BP 684
EP 698
DI 10.1016/j.icarus.2013.01.006
PG 15
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 116ZZ
UT WOS:000316923200005
ER
PT J
AU Bottke, WF
Vokrouhlicky, D
Nesvorny, D
Moore, JM
AF Bottke, William F.
Vokrouhlicky, David
Nesvorny, David
Moore, Jeffrey M.
TI Black rain: The burial of the Galilean satellites in irregular satellite
debris
SO ICARUS
LA English
DT Article
DE Ganymede; Jupiter, Satellites; Irregular satellites; Callisto; Europa
ID INFRARED MAPPING SPECTROMETER; OUTER SOLAR-SYSTEM; MAIN ASTEROID BELT;
TERRESTRIAL PLANETS; SUBSURFACE OCEAN; GIANT PLANETS; COLLISIONAL
EVOLUTION; CIRCUMPLANETARY DUST; URANIAN SATELLITES; NATURAL SATELLITES
AB Irregular satellites are dormant comet-like bodies that reside on distant prograde and retrograde orbits around the giant planets. They are likely to be captured objects. Dynamical modeling work indicates they may have been caught during a violent reshuffling of the giant planets similar to 4 Gy ago (Ga) as described by the so-called Nice model. According to this scenario, giant planet migration scattered tens of Earth masses of comet-like bodies throughout the Solar System, with some comets finding themselves near giant planets experiencing mutual encounters. In these cases, gravitational perturbations between the giant planets were often sufficient to capture the comet-like bodies onto irregular satellite-like orbits via three-body reactions. Modeling work suggests these events led to the capture of on the order of similar to 0.001 lunar masses of comet-like objects on isotropic orbits around the giant planets. Roughly half of the population was readily lost by interactions with the Kozai resonance. The remaining half found themselves on orbits consistent with the known irregular satellites. From there, the bodies experienced substantial collisional evolution, enough to grind themselves down to their current low-mass states.
Here we explore the fate of the putative irregular satellite debris in the Jupiter system. Pulverized by collisions, we hypothesize that the carbonaceous chondrite-like material was beaten into small enough particles that it could be driven toward Jupiter by Poynting-Robertson (P-R) drag forces. Assuming its mass distribution was dominated by D > 50 mu m particles, we find that >40% ended up striking the Galilean satellites. The majority were swept up by Callisto, with a factor of 3-4 and 20-30 fewer particles reaching Ganymede and Europa/b, respectively. Collision evolution models indicate most of this material arrived about 4 Ga, but some is still arriving today. We predict that Callisto, Ganymede, Europa, and Io were buried about 4 Ga by similar to 120-140 m, 25-30 m, 7-15 m, and 7-8 m of dark debris, respectively. The first two values are consistent with observations of the deepest dark lag deposits found on the most ancient terrains of Callisto and Ganymede. The rest of the debris was likely worked into the crusts of these worlds by geologic and impact processes. This suggests the debris is a plausible source of the dark lag material found in Europa's low-lying crevices. More speculatively, it is conceivable that the accreted dark particles were a significant source of organic material to Europa's subsurface ocean. (C) 2013 Elsevier Inc. All rights reserved.
C1 [Bottke, William F.; Nesvorny, David] SW Res Inst, Boulder, CO 80302 USA.
[Bottke, William F.; Nesvorny, David] NASA, Lunar Sci Inst, Boulder, CO 80302 USA.
[Vokrouhlicky, David] Charles Univ Prague, Inst Astron, CR-18000 Prague 8, Czech Republic.
[Moore, Jeffrey M.] NASA, Ames Res Ctr, Div Space Sci, Moffett Field, CA 94035 USA.
RP Bottke, WF (reprint author), SW Res Inst, 1050 Walnut St,Suite 300, Boulder, CO 80302 USA.
EM bottke@boulder.swri.edu
FU NSF's Planetary Astronomy Program; Czech Grant Agency [205/08/0064];
Czech Ministry of Education [MSM0021620860]
FX We thank Mark Buie, Carly Howett, Simone Marchi, Louise Prockter, and
John Spencer for helpful discussions that improved this paper. We also
thank referee Dan Tamayo and an anonymous referee for their constructive
and highly useful comments. Research funds for William Bottke and David
Nesvorny on this work were provided by NSF's Planetary Astronomy
Program. The work of David Vokrouhlicky was partially supported by
research Grant 205/08/0064 of the Czech Grant Agency and the Research
Program MSM0021620860 of the Czech Ministry of Education.
NR 110
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Z9 9
U1 0
U2 12
PU ACADEMIC PRESS INC ELSEVIER SCIENCE
PI SAN DIEGO
PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA
SN 0019-1035
EI 1090-2643
J9 ICARUS
JI Icarus
PD APR
PY 2013
VL 223
IS 2
BP 775
EP 795
DI 10.1016/j.icarus.2013.01.008
PG 21
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 116ZZ
UT WOS:000316923200013
ER
PT J
AU Choi, DS
Showman, AP
Vasavada, AR
Simon-Miller, AA
AF Choi, David S.
Showman, Adam P.
Vasavada, Ashwin R.
Simon-Miller, Amy A.
TI Meteorology of Jupiter's equatorial hot spots and plumes from Cassini
SO ICARUS
LA English
DT Article
DE Jupiter; Jupiter, Atmosphere; Atmospheres, Dynamics; Meteorology
ID GREAT RED SPOT; GALILEO PROBE; DYNAMICAL IMPLICATIONS; VERTICAL
STRUCTURE; MOIST CONVECTION; WHITE OVALS; ZONAL WINDS; ATMOSPHERE;
AMMONIA; CLOUDS
AB We present an updated analysis of Jupiter's equatorial meteorology from Cassini observations. For two months preceding the spacecraft's closest approach, the Imaging Science Subsystem (ISS) onboard regularly imaged the atmosphere. We created time-lapse movies from this period in order to analyze the dynamics of equatorial hot spots and their interactions with adjacent latitudes. Hot spots are relatively cloud-free regions that emit strongly at 5 mu m; improved knowledge of these features is crucial for fully understanding Galileo probe measurements taken during its descent through one. Hot spots are quasi-stable, rectangular dark areas on visible-wavelength images, with defined eastern edges that sharply contrast with surrounding clouds, but diffuse western edges serving as nebulous boundaries with adjacent equatorial plumes. Hot spots exhibit significant variations in size and shape over timescales of days and weeks. Some of these changes correspond with passing vortex systems from adjacent latitudes interacting with hot spots. Strong anticyclonic gyres present to the south and southeast of the dark areas appear to circulate into hot spots. Impressive, bright white plumes occupy spaces in between hot spots. Compact cirrus-like 'scooter' clouds flow rapidly through the plumes before disappearing within the dark areas. These clouds travel at 150-200 m s(-1), much faster than the 100 m s(-1) hot spot and plume drift speed. This raises the possibility that the scooter clouds may be more illustrative of the actual jet stream speed at these latitudes. Most previously published zonal wind profiles represent the drift speed of the hot spots at their latitude from pattern matching of the entire longitudinal image strip. If a downward branch of an equatorially-trapped Rossby wave controls the overall appearance of hot spots, however, the westward phase velocity of the wave leads to underestimates of the true jet stream speed. (C) 2013 Elsevier Inc. All rights reserved.
C1 [Choi, David S.] NASA, Goddard Space Flight Ctr, ORAU, Greenbelt, MD 20771 USA.
[Showman, Adam P.] Univ Arizona, Dept Planetary Sci, Tucson, AZ 85721 USA.
[Vasavada, Ashwin R.] CALTECH, Jet Prop Lab, Pasadena, CA 91011 USA.
[Simon-Miller, Amy A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Choi, DS (reprint author), NASA, Goddard Space Flight Ctr, ORAU, Greenbelt, MD 20771 USA.
EM david.s.choi@nasa.gov
RI Simon, Amy/C-8020-2012
OI Simon, Amy/0000-0003-4641-6186
FU NASA Jupiter Data Analysis Program [NNX09AD98G]; NASA Postdoctoral
Program at Goddard Space Flight Center; Oak Ridge Associated
Universities; NASA
FX We thank two anonymous reviewers for their comments that strengthened
this manuscript. This research was supported by a NASA Jupiter Data
Analysis Program Grant, #NNX09AD98G, and by an appointment to the NASA
Postdoctoral Program at Goddard Space Flight Center, administered by Oak
Ridge Associated Universities through a contract with NASA.
NR 36
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U1 2
U2 12
PU ACADEMIC PRESS INC ELSEVIER SCIENCE
PI SAN DIEGO
PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA
SN 0019-1035
J9 ICARUS
JI Icarus
PD APR
PY 2013
VL 223
IS 2
BP 832
EP 843
DI 10.1016/j.icarus.2013.02.001
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 116ZZ
UT WOS:000316923200017
ER
PT J
AU Polzin, KA
Adwar, JE
Hallock, AK
AF Polzin, Kurt A.
Adwar, Jake E.
Hallock, Ashley K.
TI Optimization of Electrodynamic Energy Transfer in Coilguns With
Multiple, Uncoupled Stages
SO IEEE TRANSACTIONS ON MAGNETICS
LA English
DT Article
DE Coilgun; inductive accelerators; modeling; optimization
ID INDUCTIVE THRUSTER; PERFORMANCE; DESIGN; ACCELERATION
AB A 1-D model for inductive electromagnetic acceleration of projectiles using a coilgun has been nondimensionalized to find relevant scaling parameters. The dynamic impedance parameter, representing the ratio of the resonant period of the unloaded electrical circuit to the time the projectile is electromagnetically coupled to the coil, is the scaling term that can be adjusted to optimize the electromagnetic energy transfer process. The mutual inductance profile, which represents the ability to convert potential electromagnetic energy into projectile kinetic energy, was modeled for a specific geometry using a semi-empirical function previously found suitable for cylindrical pulsed inductive plasma accelerators. Contour plots representing coilgun efficiency were generated for varying initial projectile velocity across a range of dynamic impedances. The contour plots show that below a given initial velocity a dynamic impedance parameter can be selected to maximize energy transfer to the projectile. This optimum varies as a function of the initial velocity a projectile possessed when it enters the coilgun stage. Once the contour plot is generated for a geometry it can be used to optimize the acceleration process for any stage in a coilgun if the individual coils comprising the stages are electromagnetically uncoupled from each other and the velocity of the projectile as it exits the previous stage is known.
C1 [Polzin, Kurt A.] NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA.
[Adwar, Jake E.] SUNY Stony Brook, Stony Brook, NY 11790 USA.
[Hallock, Ashley K.] NASA, Yetispace Inc, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA.
RP Polzin, KA (reprint author), NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA.
EM kurt.a.polzin@nasa.gov
NR 23
TC 3
Z9 4
U1 0
U2 9
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 0018-9464
EI 1941-0069
J9 IEEE T MAGN
JI IEEE Trans. Magn.
PD APR
PY 2013
VL 49
IS 4
BP 1453
EP 1460
DI 10.1109/TMAG.2012.2230271
PG 8
WC Engineering, Electrical & Electronic; Physics, Applied
SC Engineering; Physics
GA 115II
UT WOS:000316805400023
ER
PT J
AU Lei, JF
Goldberg, RK
AF Lei, Jih-Fen
Goldberg, Robert K.
TI Special Issue on Seventy Years of Aerospace Research and Technology
Excellence at NASA Glenn Research Center Introduction
SO JOURNAL OF AEROSPACE ENGINEERING
LA English
DT Editorial Material
C1 [Lei, Jih-Fen] NASA, Res & Technol Directorate, Glenn Res Ctr, Cleveland, OH 44135 USA.
[Goldberg, Robert K.] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA.
RP Goldberg, RK (reprint author), NASA, Glenn Res Ctr, 21000 Brookpk Rd, Cleveland, OH 44135 USA.
EM jih-fen.lei@nasa.gov; Robert.K.Goldberg@nasa.gov
NR 0
TC 0
Z9 0
U1 0
U2 6
PU ASCE-AMER SOC CIVIL ENGINEERS
PI RESTON
PA 1801 ALEXANDER BELL DR, RESTON, VA 20191-4400 USA
SN 0893-1321
J9 J AEROSPACE ENG
JI J. Aerosp. Eng.
PD APR
PY 2013
VL 26
IS 2
SI SI
BP 197
EP 201
DI 10.1061/(ASCE)AS.1943-5525.0000320
PG 5
WC Engineering, Aerospace; Engineering, Civil
SC Engineering
GA 118YR
UT WOS:000317063900001
ER
PT J
AU Reddy, DR
AF Reddy, Dhanireddy R.
TI Seventy Years of Aeropropulsion Research at NASA Glenn Research Center
SO JOURNAL OF AEROSPACE ENGINEERING
LA English
DT Article
DE Air-breathing propulsion; Gas turbine engines; Turbojet; Turbofan;
Turboprop; Energy efficiency; Environmental impact; High-speed
propulsion; Fundamental research; Technology development
AB This paper presents a brief overview of air-breathing propulsion research conducted at the National Aeronautics and Space Administration (NASA) Glenn Research Center (GRC) over the last 70 years. It includes a historical perspective of the center and its various stages of propulsion research in response to the country's different periods of crises and growth opportunities. The GRC's research and technology development covered a broad spectrum, from a short-term focus on improving the energy efficiency of aircraft engines to advancing the frontier technologies of high-speed aviation in the supersonic and hypersonic speed regimes. This paper highlights major research programs, showing their impact on industry and aircraft propulsion, and briefly discusses current research programs and future aeropropulsion technology trends in related areas. DOI: 10.1061/(ASCE)AS.1943-5525.0000312. (C) 2013 American Society of Civil Engineers.
C1 NASA, Aeropropuls Div, Glenn Res Ctr, Cleveland, OH 44135 USA.
RP Reddy, DR (reprint author), NASA, Aeropropuls Div, Glenn Res Ctr, 21000 Brookpk Rd, Cleveland, OH 44135 USA.
EM dhanireddy.r.reddy@nasa.gov
NR 29
TC 0
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U1 2
U2 18
PU ASCE-AMER SOC CIVIL ENGINEERS
PI RESTON
PA 1801 ALEXANDER BELL DR, RESTON, VA 20191-4400 USA
SN 0893-1321
J9 J AEROSPACE ENG
JI J. Aerosp. Eng.
PD APR
PY 2013
VL 26
IS 2
SI SI
BP 202
EP 217
DI 10.1061/(ASCE)AS.1943-5525.0000312
PG 16
WC Engineering, Aerospace; Engineering, Civil
SC Engineering
GA 118YR
UT WOS:000317063900002
ER
PT J
AU Huff, DL
AF Huff, Dennis L.
TI NASA Glenn's Contributions to Aircraft Engine Noise Research
SO JOURNAL OF AEROSPACE ENGINEERING
LA English
DT Article
DE Turbofan; Turbojet; Aircraft engine noise; Acoustics; Aeroacoustics;
Fans; Jets; Turbomachinery; Noise reduction
AB This paper reviews all engine noise research conducted at the National Aeronautics and Space Administration (NASA) Glenn Research Center over the last 70 years. The review includes a historical perspective of the center and the facilities used to conduct the research. Major NASA noise research programs are highlighted, showing their impact on the industry and on the development of aircraft noise reduction technology. Noise reduction trends are discussed, and future aircraft concepts are presented. Results show that, since the 1960s, the average perceived noise level has been reduced by about 20 dB. Studies show that, depending on the size of the airport, the aircraft fleet mix, and the actual growth in air travel, another 15-17 dB is required to achieve NASA's long-term goal of providing technologies to limit objectionable noise to the boundaries of an average airport. DOI: 10.1061/(ASCE)AS.1943-5525.0000283. (C) 2013 American Society of Civil Engineers.
C1 NASA, Aeropropuls Div, Glenn Res Ctr, Cleveland, OH 44135 USA.
RP Huff, DL (reprint author), NASA, Aeropropuls Div, Glenn Res Ctr, 21000 Brookpk Rd, Cleveland, OH 44135 USA.
EM dennis.l.huff@nasa.gov
NR 93
TC 1
Z9 1
U1 0
U2 13
PU ASCE-AMER SOC CIVIL ENGINEERS
PI RESTON
PA 1801 ALEXANDER BELL DR, RESTON, VA 20191-4400 USA
SN 0893-1321
J9 J AEROSPACE ENG
JI J. Aerosp. Eng.
PD APR
PY 2013
VL 26
IS 2
SI SI
BP 218
EP 250
DI 10.1061/(ASCE)AS.1943-5525.0000283
PG 33
WC Engineering, Aerospace; Engineering, Civil
SC Engineering
GA 118YR
UT WOS:000317063900003
ER
PT J
AU Chang, CT
Tacina, K
Lee, C
Bulzan, D
Hicks, Y
Liu, NS
Lee, J
AF Chang, C. T.
Tacina, K.
Lee, C.
Bulzan, D.
Hicks, Y.
Liu, N. -S.
Lee, J.
TI NASA Glenn Combustion Research for Aeronautical Propulsion
SO JOURNAL OF AEROSPACE ENGINEERING
LA English
DT Article
DE Combustion; Combustor concept; Fuel injection; Alternate fuel; Optical
diagnostic; CFD; Hypersonic propulsion
ID SUBSONIC CROSS-FLOW; MULTIPLE JETS; PRESSURE
AB NASA Glenn Research Center (GRC) has been involved in a wide range of combustion research topics in combustor concept research, component technology development, and enabling technology development to provide enabling technologies for flight regimes from subsonic to hypersonic. These research efforts were carried out by NASA and industrial and academic partners through a range of NASA fundamental research and focused programs. These synergistic efforts in fuel injection, flame stabilization, combustion physics, and ignition studies have resulted in combustor concept changes that resulted in much cleaner-burning modern jet engines. New computational tools, optical diagnostics, fuels, and fuel conditioning technology are being currently used to develop a better understanding of the complex processes occurring in combustion systems for a range of future propulsion systems. DOI: 10.1061/(ASCE)AS.1943-5525.0000289. (C) 2013 American Society of Civil Engineers.
C1 [Chang, C. T.; Tacina, K.; Bulzan, D.; Hicks, Y.; Liu, N. -S.; Lee, J.] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA.
[Lee, C.] NASA, Combust Branch, Glenn Res Ctr, Cleveland, OH 44135 USA.
RP Chang, CT (reprint author), NASA, Glenn Res Ctr, Cleveland, OH 44135 USA.
EM Clarence.T.Chang@nasa.gov; Kathleen.M.Tacina@nasa.gov;
Chi-ming.Lee-1@nasa.gov; Dan.L.Bulzan@nasa.gov;
Yolanda.R.Hicks@nasa.gov; Nan-suey.Liu-1@nasa.gov; Jinho.Lee-1@nasa.gov
NR 104
TC 1
Z9 1
U1 2
U2 8
PU ASCE-AMER SOC CIVIL ENGINEERS
PI RESTON
PA 1801 ALEXANDER BELL DR, RESTON, VA 20191-4400 USA
SN 0893-1321
J9 J AEROSPACE ENG
JI J. Aerosp. Eng.
PD APR
PY 2013
VL 26
IS 2
SI SI
BP 251
EP 259
DI 10.1061/(ASCE)AS.1943-5525.0000289
PG 9
WC Engineering, Aerospace; Engineering, Civil
SC Engineering
GA 118YR
UT WOS:000317063900004
ER
PT J
AU Potapczuk, MG
AF Potapczuk, Mark G.
TI Aircraft Icing Research at NASA Glenn Research Center
SO JOURNAL OF AEROSPACE ENGINEERING
LA English
DT Article
DE Aircraft icing
AB The National Aeronautics and Space Administration Glenn Research Center (GRC; and its predecessor organizations) has been and continues to be a focal point for research in the field of aircraft icing. This paper provides a historical perspective on the contributions that GRC research has made to the field, as well as a synopsis of the current research being conducted at the center. The GRC's icing research has been comprehensive, covering the characterization of the icing environment, investigations into the physics of ice accretion on aircraft surfaces, studies of the impact of icing on aircraft aerodynamics and engine performance, icing instrumentation development, and simulation of ice growth on aircraft using wind tunnels and computational methods. This research has led to improved safety for flight in icing conditions through contributions to the development of icing regulations; a greater understanding of the effects of ice accretion; and the development of experimental and computational methods to aid in the design of aircraft and aircraft subsystems (including ice protection systems) that can operate safely in an icing environment. DOI: 10.1061/(ASCE)AS.1943-5525.0000322. (C) 2013 American Society of Civil Engineers.
C1 NASA, Glenn Res Ctr, Cleveland, OH 44135 USA.
RP Potapczuk, MG (reprint author), NASA, Glenn Res Ctr, 21000 Brookpk Rd, Cleveland, OH 44135 USA.
EM Mark.G.Potapczuk@nasa.gov
NR 102
TC 5
Z9 6
U1 3
U2 17
PU ASCE-AMER SOC CIVIL ENGINEERS
PI RESTON
PA 1801 ALEXANDER BELL DR, RESTON, VA 20191-4400 USA
SN 0893-1321
J9 J AEROSPACE ENG
JI J. Aerosp. Eng.
PD APR
PY 2013
VL 26
IS 2
SI SI
BP 260
EP 276
DI 10.1061/(ASCE)AS.1943-5525.0000322
PG 17
WC Engineering, Aerospace; Engineering, Civil
SC Engineering
GA 118YR
UT WOS:000317063900005
ER
PT J
AU Liou, MS
Povinelli, LA
AF Liou, Meng-Sing
Povinelli, Louis A.
TI Computational Fluid Dynamics: NASA Glenn Research Center's Legacy and
Contributions
SO JOURNAL OF AEROSPACE ENGINEERING
LA English
DT Article
DE Numerical methods; Turbulence modeling; Inlet and nozzle; Aeroacoustics;
Combustion; Compressor; Turbine heat transfer; Engine system simulation;
Validation; CFD codes; Multidisciplinary analysis; Design optimization
ID TIME CONSERVATION ELEMENT; DIFFERENCE-SCHEMES; SPLITTING SCHEME;
NAVIER-STOKES; JET FLOW; ACCURATE; ROTOR; AUSM(+)-UP; EQUATIONS; SYSTEMS
AB Development and contributions to computational fluid dynamics (CFD) at the National Aeronautics and Space Administration (NASA) Glenn Research Center (GRC) during the period from 1947 to the present are reviewed in five categories: numerical methods, physical modeling, CFD codes development, CFD validation and engineering applications, and multidisciplinary design optimization. Some representative results in applications to aero and propulsion systems are included to illustrate the developed capabilities. GRC has a long history of investing resources to develop these key subject matters, with an interest in a wide range of applications, primarily focusing on propulsion-related technologies and concepts. The evolved CFD capabilities have enabled simulations of complex three-dimensional flow fields for engine components and integrated configurations, as illustrated in this article. This article is intended to give a useful, albeit noncomplete, overview into GRC's work in CFD. DOI: 10.1061/(ASCE)AS.1943-5525.0000295. (C) 2013 American Society of Civil Engineers.
C1 [Liou, Meng-Sing; Povinelli, Louis A.] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA.
RP Liou, MS (reprint author), NASA, Glenn Res Ctr, MS 5-11, Cleveland, OH 44135 USA.
EM meng-sing.liou@nasa.gov
NR 97
TC 1
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U1 0
U2 24
PU ASCE-AMER SOC CIVIL ENGINEERS
PI RESTON
PA 1801 ALEXANDER BELL DR, RESTON, VA 20191-4400 USA
SN 0893-1321
J9 J AEROSPACE ENG
JI J. Aerosp. Eng.
PD APR
PY 2013
VL 26
IS 2
SI SI
BP 277
EP 287
DI 10.1061/(ASCE)AS.1943-5525.0000295
PG 11
WC Engineering, Aerospace; Engineering, Civil
SC Engineering
GA 118YR
UT WOS:000317063900006
ER
PT J
AU Lyons, VJ
AF Lyons, Valerie J.
TI Power and Propulsion at NASA Glenn Research Center: Historic Perspective
of Major Accomplishments
SO JOURNAL OF AEROSPACE ENGINEERING
LA English
DT Article
DE Power; Propulsion; Space power; NASA history; Lewis Research Center;
Alternative energy; Solar power; Nuclear space power; Electric
propulsion; Stirling convertors
ID SYSTEM
AB Propulsion and power have long been core competencies of the National Aeronautics and Space Administration (NASA) Glenn Research Center (GRC). At the dawn of the space era, the center brought key propulsion and power technology to support spacecraft development. This paper serves as an introduction to a series of papers describing the highlights of the GRC's power and propulsion research and development efforts. The power papers cover solar and nuclear power generation and energy conversion, energy storage (focusing on batteries, flywheels, and fuel cells), power systems, and power management and distribution. The propulsion papers cover chemical propulsion, cryogenic propellant systems, electric propulsion, and nuclear thermal rocket propulsion. Each paper addresses some history, current efforts, and future plans for each of the technology areas. DOI: 10.1061/(ASCE)AS.1943-5525.0000315. (C) 2013 American Society of Civil Engineers.
C1 NASA, Power & In Space Prop Div, Glenn Res Ctr, Cleveland, OH 44135 USA.
RP Lyons, VJ (reprint author), NASA, Power & In Space Prop Div, Glenn Res Ctr, 21000 Brookpk Rd, Cleveland, OH 44135 USA.
EM Valerie.J.Lyons@nasa.gov
NR 39
TC 0
Z9 0
U1 5
U2 49
PU ASCE-AMER SOC CIVIL ENGINEERS
PI RESTON
PA 1801 ALEXANDER BELL DR, RESTON, VA 20191-4400 USA
SN 0893-1321
J9 J AEROSPACE ENG
JI J. Aerosp. Eng.
PD APR
PY 2013
VL 26
IS 2
SI SI
BP 288
EP 299
DI 10.1061/(ASCE)AS.1943-5525.0000315
PG 12
WC Engineering, Aerospace; Engineering, Civil
SC Engineering
GA 118YR
UT WOS:000317063900007
ER
PT J
AU Patterson, MJ
Sovey, JS
AF Patterson, Michael J.
Sovey, James S.
TI History of Electric Propulsion at NASA Glenn Research Center: 1956 to
Present
SO JOURNAL OF AEROSPACE ENGINEERING
LA English
DT Article
DE Electric propulsion; Arcjets; Hall effect thrusters; Ion thrusters;
Glenn Research Center; Lewis Research Center
ID ION PROPULSION; THRUSTER; SPACECRAFT
AB This paper provides a brief overview of the history of electric propulsion (EP) at the National Aeronautics and Space Administration (NASA) Glenn Research Center (GRC). Since the inception of EP technology, GRC has played a pivotal role in developing the technology and transitioning it to flight. Research and development efforts by GRC's employees, grantees, and contractors brought operational EP systems to commercial satellites in the early 1990s and to NASA and other government agency missions starting in the late 1990s. GRC's early construction of unique EP test infrastructure and NASA's and GRC's sustained investments in EP research and development over several decades were strategic in the creation of technologies that continue to greatly benefit the competitiveness and capabilities of U. S. space systems and missions. DOI: 10.1061/(ASCE)AS.1943-5525.0000304. (C) 2013 American Society of Civil Engineers.
C1 [Patterson, Michael J.] NASA, In Space Prop, Glenn Res Ctr, Cleveland, OH 44135 USA.
[Sovey, James S.] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA.
RP Patterson, MJ (reprint author), NASA, In Space Prop, Glenn Res Ctr, Cleveland, OH 44135 USA.
EM michael.j.patterson@nasa.gov
NR 67
TC 5
Z9 6
U1 2
U2 33
PU ASCE-AMER SOC CIVIL ENGINEERS
PI RESTON
PA 1801 ALEXANDER BELL DR, RESTON, VA 20191-4400 USA
SN 0893-1321
J9 J AEROSPACE ENG
JI J. Aerosp. Eng.
PD APR
PY 2013
VL 26
IS 2
SI SI
BP 300
EP 316
DI 10.1061/(ASCE)AS.1943-5525.0000304
PG 17
WC Engineering, Aerospace; Engineering, Civil
SC Engineering
GA 118YR
UT WOS:000317063900008
ER
PT J
AU Linne, DL
Aukerman, CA
Palaszewski, BA
AF Linne, Diane L.
Aukerman, Carl A.
Palaszewski, Bryan A.
TI Chemical Propulsion: Greater than 60 Years of Leadership and Innovation
at NASA Glenn Research Center
SO JOURNAL OF AEROSPACE ENGINEERING
LA English
DT Article
DE Aerospace engineering; Engines; Experimentation; History; Research
AB The National Aeronautics and Space Administration (NASA) Glenn Research Center (GRC) was built during World War II with the primary objective of catching up with the Germans in jet engine technology. A decade later, it seemed only natural that these same aeropropulsion engineers would progress into the largely unexplored field of space chemical propulsion. Starting before the launch of Sputnik set off the great space race, researchers at the GRC were testing and flying cryogenic hydrogen-fueled engines that were an eventual key to the success of the Apollo manned missions to the moon. In the 60 years since this first foray into chemical propulsion, engineers at the GRC have made countless innovations and contributions to every component of rocket engine technology. From energetic propellants to green fuels, from innovative metallic alloys to ceramic composites, from seals and bearings to igniters and injectors, and from upper stages and satellites to launch vehicles and planetary landers, the dedicated and creative people at the GRC have propelled the United States to the forefront of space exploration and continue to work toward an even more exciting future. Some of the highlights of this illustrious and ongoing journey are explored in this paper. DOI: 10.1061/(ASCE)AS.1943-5525.0000303. (C) 2013 American Society of Civil Engineers.
C1 [Linne, Diane L.; Aukerman, Carl A.; Palaszewski, Bryan A.] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA.
RP Linne, DL (reprint author), NASA, Glenn Res Ctr, 21000 Brookpk Rd, Cleveland, OH 44135 USA.
EM diane.l.linne@nasa.gov; auk4@aol.com; bryan.a.palaszewski@nasa.gov
NR 74
TC 2
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U1 3
U2 26
PU ASCE-AMER SOC CIVIL ENGINEERS
PI RESTON
PA 1801 ALEXANDER BELL DR, RESTON, VA 20191-4400 USA
SN 0893-1321
J9 J AEROSPACE ENG
JI J. Aerosp. Eng.
PD APR
PY 2013
VL 26
IS 2
SI SI
BP 317
EP 333
DI 10.1061/(ASCE)AS.1943-5525.0000303
PG 17
WC Engineering, Aerospace; Engineering, Civil
SC Engineering
GA 118YR
UT WOS:000317063900009
ER
PT J
AU Borowski, SK
AF Borowski, Stanley K.
TI Nuclear Thermal Propulsion: Past Accomplishments, Present Efforts, and a
Look Ahead
SO JOURNAL OF AEROSPACE ENGINEERING
LA English
DT Article
DE Nuclear thermal rocket; NTR; Rover/Nuclear Engine for Rocket Vehicle
Applications (NERVA); Spacecraft; Human Moon Mars exploration
AB The National Aeronautics and Space Administration (NASA) Glenn Research Center (GRC) has been actively involved in nuclear thermal propulsion (NTP) technology development, mission, engine, and vehicle design dating back to the Rover and Nuclear Engine for Rocket Vehicle Applications programs. This technology was successfully developed in over 20 rocket/reactor tests, which demonstrated a wide range of thrust levels, high-temperature fuel, sustained engine operation, accumulated time at full power, and restart capability-everything required for a human mission to Mars. Furthermore, NTP requires no large technology scale-up. The smallest engine tested during the Rover program-the Pewee Engine-is sufficient for this when used in a clustered engine arrangement. The GRC has led every major study involving NTP since the late 1980s and has helped quantify the evolution and growth potential of the nuclear thermal rocket (NTR), which includes the bimodal and liquid-oxygen- (LOX-) augmented NTR concepts. In NASA's recent Mars Design Reference Architecture (DRA) study, NTP reduced total mission mass over 400 t compared with chemical propulsion. Human missions to the Moon and near-Earth asteroids are also enhanced using NTP. In 2011, NASA restarted an NTP technology demonstration effort that is continuing under the Nuclear Cryogenic Propulsion Stage project, which began in 2012. Ground demonstrations of a small, scalable NTR by 2020 are envisioned, with a flight demonstration shortly thereafter. DOI: 10.1061/(ASCE)AS.1943-5525.0000313. (C) 2013 American Society of Civil Engineers.
C1 NASA, Prop & Control Syst Anal Branch, Glenn Res Ctr, Cleveland, OH 44135 USA.
RP Borowski, SK (reprint author), NASA, Prop & Control Syst Anal Branch, Glenn Res Ctr, 21000 Brookpk Rd, Cleveland, OH 44135 USA.
EM stanley.k.borowski@nasa.gov
NR 34
TC 1
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U1 2
U2 41
PU ASCE-AMER SOC CIVIL ENGINEERS
PI RESTON
PA 1801 ALEXANDER BELL DR, RESTON, VA 20191-4400 USA
SN 0893-1321
J9 J AEROSPACE ENG
JI J. Aerosp. Eng.
PD APR
PY 2013
VL 26
IS 2
SI SI
BP 334
EP 342
DI 10.1061/(ASCE)AS.1943-5525.0000313
PG 9
WC Engineering, Aerospace; Engineering, Civil
SC Engineering
GA 118YR
UT WOS:000317063900010
ER
PT J
AU Meyer, ML
Chato, DJ
Plachta, DW
Zimmerli, GA
Barsi, SJ
Van Dresar, NT
Moder, JP
AF Meyer, Michael L.
Chato, David J.
Plachta, David W.
Zimmerli, Gregory A.
Barsi, Stephen J.
Van Dresar, Neil T.
Moder, Jeffrey P.
TI Mastering Cryogenic Propellants
SO JOURNAL OF AEROSPACE ENGINEERING
LA English
DT Article
DE Space exploration; Spacecraft; Aerospace engineering; Research; Fluid
dynamics; Thermodynamics; Tanks
AB The National Aeronautics and Space Administration (NASA) Glenn Research Center (GRC) began experimentation with cryogenic propellants in the early 1950s to understand the potential of these high-performance propellants for use in liquid propellant rocket engines. Supporting these tests required learning how to both design cryogenic systems and develop procedures to safely and reliably work with cryogenic fuels and oxidizers. This early work led to the development of a skill set that has been core to the center ever since. When NASA was formed and the exploration missions were defined, it became clear that the ability to use cryogenic propellants in the thermal and microgravity environment of space was critical to mission success, and the agency was tasked with enabling this capability. To support development of the Centaur upper stage and the Saturn S-IVB stage, GRC researchers and engineers initiated extensive technology development for the in-space application of cryogenic fluid management (CFM). These initial efforts addressed basic requirements of propellant slosh, settling, and short-term storage/pressure control. Over the ensuing years, the NASA GRC has advanced CFM technologies to enable more reliable and capable upper stages. Today, these CFM technologies are on the brink of enabling long-duration in-space cryogenic propulsion stages and cryogenic propellant depots. DOI: 10.1061/(ASCE)AS.1943-5525.0000297. (C) 2013 American Society of Civil Engineers.
C1 [Meyer, Michael L.] NASA, Power & In Space Prop Div, Glenn Res Ctr, Cleveland, OH 44135 USA.
[Chato, David J.; Plachta, David W.; Zimmerli, Gregory A.; Barsi, Stephen J.; Van Dresar, Neil T.; Moder, Jeffrey P.] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA.
RP Meyer, ML (reprint author), NASA, Power & In Space Prop Div, Glenn Res Ctr, 21000 Brookpk Rd, Cleveland, OH 44135 USA.
EM michael.l.meyer@nasa.gov; david.j.chato@nasa.gov;
david.w.plachta@nasa.gov; greg.zimmerli@nasa.gov;
stephen.j.barsi@nasa.gov; neil.t.vandresar@nasa.gov;
jeffrey.p.moder@nasa.gov
RI Chato, David/B-2698-2013
OI Chato, David/0000-0003-2990-0646
NR 69
TC 3
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U1 1
U2 19
PU ASCE-AMER SOC CIVIL ENGINEERS
PI RESTON
PA 1801 ALEXANDER BELL DR, RESTON, VA 20191-4400 USA
SN 0893-1321
J9 J AEROSPACE ENG
JI J. Aerosp. Eng.
PD APR
PY 2013
VL 26
IS 2
SI SI
BP 343
EP 351
DI 10.1061/(ASCE)AS.1943-5525.0000297
PG 9
WC Engineering, Aerospace; Engineering, Civil
SC Engineering
GA 118YR
UT WOS:000317063900011
ER
PT J
AU Mason, LS
AF Mason, Lee S.
TI Dynamic Energy Conversion: Vital Technology for Space Nuclear Power
SO JOURNAL OF AEROSPACE ENGINEERING
LA English
DT Article
DE Space; Nuclear power; Energy conversion; Brayton; Stirling
AB The National Aeronautics and Space Administration Glenn Research Center (GRC) has an extensive history in dynamic energy conversion dating back to the early 1960s. This legacy puts the GRC at the forefront of nuclear power systems using thermodynamic power cycles such as Stirling and Brayton. The advantages of dynamic energy conversion include high efficiency, long life, and scalability to high power. These attributes make Brayton and Stirling power cycles an ideal solution for nuclear energy conversion. DOI: 10.1061/(ASCE)AS.1943-5525.0000318. (C) 2013 American Society of Civil Engineers.
C1 NASA, Thermal Energy Convers Branch, Glenn Res Ctr, Cleveland, OH USA.
RP Mason, LS (reprint author), NASA, Thermal Energy Convers Branch, Glenn Res Ctr, 21000 Brookpk Rd, Cleveland, OH USA.
EM lee.s.mason@nasa.gov
NR 48
TC 2
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U1 0
U2 8
PU ASCE-AMER SOC CIVIL ENGINEERS
PI RESTON
PA 1801 ALEXANDER BELL DR, RESTON, VA 20191-4400 USA
SN 0893-1321
J9 J AEROSPACE ENG
JI J. Aerosp. Eng.
PD APR
PY 2013
VL 26
IS 2
SI SI
BP 352
EP 360
DI 10.1061/(ASCE)AS.1943-5525.0000318
PG 9
WC Engineering, Aerospace; Engineering, Civil
SC Engineering
GA 118YR
UT WOS:000317063900012
ER
PT J
AU Reid, CM
Miller, TB
Hoberecht, MA
Loyselle, PL
Taylor, LM
Farmer, SC
Jansen, RH
AF Reid, Concha M.
Miller, Thomas B.
Hoberecht, Mark A.
Loyselle, Patricia L.
Taylor, Linda M.
Farmer, Serene C.
Jansen, Ralph H.
TI History of Electrochemical and Energy Storage Technology Development at
NASA Glenn Research Center
SO JOURNAL OF AEROSPACE ENGINEERING
LA English
DT Article
DE Energy storage; Electric power; Mechanical systems; Spacecraft; Space
stations; Energy; Satellites; Energy sources
AB The National Aeronautics and Space Administration Glenn Research Center (GRC) has a rich heritage of developing electrochemical technologies and energy storage systems for aerospace. Primary and rechargeable batteries, fuel cells, flywheels, and regenerative fuel cells are among the GRC's portfolio of energy storage devices and primary power systems. These technologies have been developed for missions and applications such as low Earth orbit and geosynchronous Earth orbit satellites, space shuttle, astronaut spacesuit, International Space Station, landers and rovers, and lunar and planetary habitats. The desire for lower mass, lower volume, higher efficiency, and more reliable power systems has most often been the driving force behind the development of these technologies. Often, as with fuel cells for the early Gemini and Apollo missions, development of the technology has been mission enabling. Although many of these technologies were initially developed for applications in space, the existence of such capabilities or development successes at GRC has led to their adoption for terrestrial uses or further research and development for terrestrial applications, including electric vehicles, unmanned aerial and underwater vehicles, and all-electric aircraft. This paper discusses the history of and the current research and development at the GRC in electrochemical and energy storage technologies. The future outlook for each of these technologies is also addressed. DOI: 10.1061/(ASCE)AS.1943-5525.0000323. (C) 2013 American Society of Civil Engineers.
C1 [Reid, Concha M.; Miller, Thomas B.; Hoberecht, Mark A.; Loyselle, Patricia L.; Taylor, Linda M.; Farmer, Serene C.; Jansen, Ralph H.] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA.
RP Reid, CM (reprint author), NASA, Glenn Res Ctr, 21000 Brookpk Rd, Cleveland, OH 44135 USA.
EM concha.m.reid@nasa.gov; thomas.b.miller@nasa.gov;
mark.a.hoberecht@nasa.gov; patricia.l.loyselle@nasa.gov;
linda.m.taylor@nasa.gov; serene.c.farmer@nasa.gov;
ralph.h.jansen@nasa.gov
NR 58
TC 3
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U1 2
U2 49
PU ASCE-AMER SOC CIVIL ENGINEERS
PI RESTON
PA 1801 ALEXANDER BELL DR, RESTON, VA 20191-4400 USA
SN 0893-1321
J9 J AEROSPACE ENG
JI J. Aerosp. Eng.
PD APR
PY 2013
VL 26
IS 2
SI SI
BP 361
EP 371
DI 10.1061/(ASCE)AS.1943-5525.0000323
PG 11
WC Engineering, Aerospace; Engineering, Civil
SC Engineering
GA 118YR
UT WOS:000317063900013
ER
PT J
AU Seng, GT
Zeller, MV
Ramos, CT
AF Seng, Gary T.
Zeller, Mary V.
Ramos, Calvin T.
TI Introduction to the Communications, Instrumentation, and Controls
Division
SO JOURNAL OF AEROSPACE ENGINEERING
LA English
DT Article
DE Instrumentation; Harsh environment sensors; High-temperature
electronics; Turbine engine controls; Engine system dynamics;
Aerocommunications; Space communications technology; RF and optical
communications; Digital communications; Networking
AB This paper explores the organizational history of the three core discipline areas currently residing within the Communications, Instrumentation, and Controls Division, which are harsh environment instrumentation/sensors/electronics, turbine engine controls and systems dynamics, and aerospace communications technology. Division and selected branch management will be identified by discipline in chronological order. In the second section, current division research areas will be listed by branch. Finally, future progress in the key disciplines is discussed by describing near-term future work and projecting a long-term future state beyond the horizon. DOI: 10.1061/(ASCE)AS.1943-5525.0000311. (C) 2013 American Society of Civil Engineers.
C1 [Seng, Gary T.] NASA, Commun Instrumentat & Controls Div, Glenn Res Ctr, Cleveland, OH 44135 USA.
[Zeller, Mary V.; Ramos, Calvin T.] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA.
RP Seng, GT (reprint author), NASA, Commun Instrumentat & Controls Div, Glenn Res Ctr, 21000 Brookpk Rd, Cleveland, OH 44135 USA.
EM gary.t.seng@nasa.gov; mary.v.zeller@nasa.gov; calvin.t.ramos@nasa.gov
NR 12
TC 0
Z9 0
U1 0
U2 2
PU ASCE-AMER SOC CIVIL ENGINEERS
PI RESTON
PA 1801 ALEXANDER BELL DR, RESTON, VA 20191-4400 USA
SN 0893-1321
J9 J AEROSPACE ENG
JI J. Aerosp. Eng.
PD APR
PY 2013
VL 26
IS 2
SI SI
BP 372
EP 376
DI 10.1061/(ASCE)AS.1943-5525.0000311
PG 5
WC Engineering, Aerospace; Engineering, Civil
SC Engineering
GA 118YR
UT WOS:000317063900014
ER
PT J
AU Ramos, C
Fujikawa, G
Jordan, J
Miranda, FA
Ponchak, D
Pouch, JJ
Wallett, TM
AF Ramos, Calvin
Fujikawa, Gene
Jordan, Jennifer
Miranda, Felix A.
Ponchak, Denise
Pouch, John J.
Wallett, Thomas M.
TI Communications Research and Development at NASA Glenn Research Center
SO JOURNAL OF AEROSPACE ENGINEERING
LA English
DT Article
DE Radiofrequency (RF) communications; Optical communications; Digital
communications; Antennas and propagation; Navigation; Networking
protocols; Traveling-wave tube amplifiers; Communications architectures
ID TRAVELING-WAVE TUBES
AB Over the last several decades, the National Aeronautics and Space Administration (NASA) Glenn Research Center (GRC), formerly Lewis Research Center (LeRC) has performed research and technology development of aeronautic- and space-based communications in support of NASA and the nation. In the 1970s, GRC partnered with the Canadian Department of Communications through the Communications Technology Satellite (CTS) Project, in which GRC researchers were responsible for the development of critical technology components, such as the high-power, traveling-wave tube amplifier (TWTA), thereby pioneering the surge of television channels via satellite. For its efforts, LeRC was awarded an Emmy by the television industry. The decade of the 1980s served as a period for technology development that culminated in the launch of the Advanced Communications Technology Satellite (ACTS) in 1993. The ACTS demonstration of spot beam antenna technology resulted in an overall increase of efficiency in satellite communications. In the latter part of the 1990s and until today, GRC research engineers have continued to conduct research and technology development in multiple domains. The primary focus of this article is to introduce the reader to the long heritage at GRC in communications research and development through the CTS and ACTS projects and delve into specific technology areas following the ACTS Project to today in support of high-data rate communications. DOI: 10.1061/(ASCE)AS.19435525.0000316. (C) 2013 American Society of Civil Engineers.
C1 [Ramos, Calvin; Fujikawa, Gene; Ponchak, Denise] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA.
[Jordan, Jennifer] NASA, Electron & Optoelect Devices Branch, Glenn Res Ctr, Cleveland, OH 44135 USA.
[Miranda, Felix A.; Pouch, John J.; Wallett, Thomas M.] NASA, Antenna & Opt Syst Branch, Glenn Res Ctr, Cleveland, OH 44135 USA.
RP Ramos, C (reprint author), NASA, Glenn Res Ctr, Cleveland, OH 44135 USA.
EM Calvin.T.Ramos@grc.nasa.gov; Gene.Fujikawa@nasa.gov;
Jennifer.L.Jordan@nasa.gov; Felix.A.Miranda@nasa.gov;
Denise.S.Ponchak@nasa.gov; John.J.Pouch@nasa.gov;
Thomas.M.Wallett@nasa.gov
NR 52
TC 0
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U1 0
U2 8
PU ASCE-AMER SOC CIVIL ENGINEERS
PI RESTON
PA 1801 ALEXANDER BELL DR, RESTON, VA 20191-4400 USA
SN 0893-1321
J9 J AEROSPACE ENG
JI J. Aerosp. Eng.
PD APR
PY 2013
VL 26
IS 2
SI SI
BP 377
EP 394
DI 10.1061/(ASCE)AS.1943-5525.0000316
PG 18
WC Engineering, Aerospace; Engineering, Civil
SC Engineering
GA 118YR
UT WOS:000317063900015
ER
PT J
AU Baaklini, GY
AF Baaklini, George Y.
TI Optical Instrumentation and Nondestructive Evaluation Branch Research
and Technology Advances at NASA Glenn Research Center since 1941
SO JOURNAL OF AEROSPACE ENGINEERING
LA English
DT Article
DE Optical instrumentation; Nondestructive evaluation; Laser diagnostics;
Flight electronics; Health monitoring; Rayleigh scattering; Particle
imaging velocimetry; Fiber optics; Luminescent coatings; Tomography;
Ultrasonics; Remote sensing; Engine icing
ID RAYLEIGH-SCATTERING; COMPUTED-TOMOGRAPHY; ACOUSTO-ULTRASONICS;
COMPOSITES; VELOCIMETRY; SYSTEM; DAMAGE; MARS
AB This paper is a transitory decadal overview capturing the current research and technology accomplishments that are being developed by the Optical Instrumentation and Nondestructive Evaluation (NDE) Branch at the National Aeronautics and Space Administration (NASA) Glenn Research Center (GRC). The emphasis is on the latest GRC research and technology advances with a brief discussion of the history and technical background of optical instrumentation since the 1940s, NDE sciences and methods since the 1970s, fiber optics since the 1980s, space-qualified instrumentation since the 1990s, and propulsion health monitoring since the beginning of the current century. This paper also identifies and describes recent and future technical directions based on/guided by current NASA strategic and GRC and NASA project implementation plans. DOI: 10.1061/(ASCE)AS.1943-5525.0000305. (C) 2013 American Society of Civil Engineers.
C1 NASA, Opt Instrumentat & NDE Branch, Glenn Res Ctr, Cleveland, OH 44135 USA.
RP Baaklini, GY (reprint author), NASA, Opt Instrumentat & NDE Branch, Glenn Res Ctr, 21000 Brookpk Rd, Cleveland, OH 44135 USA.
EM george.y.baaklini@nasa.gov
NR 79
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U1 1
U2 18
PU ASCE-AMER SOC CIVIL ENGINEERS
PI RESTON
PA 1801 ALEXANDER BELL DR, RESTON, VA 20191-4400 USA
SN 0893-1321
EI 1943-5525
J9 J AEROSPACE ENG
JI J. Aerosp. Eng.
PD APR
PY 2013
VL 26
IS 2
SI SI
BP 395
EP 408
DI 10.1061/(ASCE)AS.1943-5525.0000305
PG 14
WC Engineering, Aerospace; Engineering, Civil
SC Engineering
GA 118YR
UT WOS:000317063900016
ER
PT J
AU Matus, LG
AF Matus, Lawrence G.
TI Instrumentation for Aerospace Applications: Electronic-Based
Technologies
SO JOURNAL OF AEROSPACE ENGINEERING
LA English
DT Article
DE Instrumentation; Sensors; Electronic devices; Microfabrication; High
temperature
ID DEGREES-C; TEMPERATURE
AB Throughout the 70-year history of the National Aeronautics and Space Administration (NASA) Glenn Research Center (GRC), instrumentation engineers have provided measurement methods and devices necessary to support ongoing and future aeropropulsion research and development efforts. On occasion, routine instrumentation approaches are perfectly suited for the task at hand. However, as propulsion components and systems become more complex through the incorporation of new materials and higher temperature operation, modifications to traditional instrumentation methods or entirely new methods are necessary. This paper provides a glimpse of the core electronic-based instrumentation methods developed throughout the years to measure temperature, strain, pressure, heat flux, and chemical gas species and describes how these methods are evolving to meet the instrumentation challenges of high-performance propulsion systems. It is clear that future aeropropulsion systems will operate at higher temperatures and require more onboard electronics for health monitoring and control functions. For this reason, a significant effort in high-temperature electronics based on the wide-bandgap semiconductor silicon carbide was initiated and has demonstrated several world's first electronic sensors and devices operating at 600 degrees C. It is concluded that electronic-based sensors and devices will continuously be pushed to meet the needs of increasingly harsher environment measurements. DOI: 10.1061/(ASCE)AS.1943-5525.0000302. (C) 2013 American Society of Civil Engineers.
C1 NASA, Sensors & Elect Branch, Glenn Res Ctr, Cleveland, OH 44135 USA.
RP Matus, LG (reprint author), NASA, Sensors & Elect Branch, Glenn Res Ctr, 21000 Brookpk Rd, Cleveland, OH 44135 USA.
EM Lawrence.G.Matus@nasa.gov
NR 65
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U1 0
U2 15
PU ASCE-AMER SOC CIVIL ENGINEERS
PI RESTON
PA 1801 ALEXANDER BELL DR, RESTON, VA 20191-4400 USA
SN 0893-1321
J9 J AEROSPACE ENG
JI J. Aerosp. Eng.
PD APR
PY 2013
VL 26
IS 2
SI SI
BP 409
EP 421
DI 10.1061/(ASCE)AS.1943-5525.0000302
PG 13
WC Engineering, Aerospace; Engineering, Civil
SC Engineering
GA 118YR
UT WOS:000317063900017
ER
PT J
AU Garg, S
AF Garg, Sanjay
TI Aircraft Turbine Engine Control Research at NASA Glenn Research Center
SO JOURNAL OF AEROSPACE ENGINEERING
LA English
DT Article
DE Gas turbine engines; Engine control; Engine performance; Robust control;
Fault detection control; Diagnostics; Dynamic modeling
ID COMPRESSOR; STALL
AB This paper provides an overview of the aircraft turbine engine control research at NASA Glenn Research Center (GRC). A brief introduction to the engine control problem is first provided with a description of the state-of-the-art control law structure. A historical aspect of engine control development since the 1940s is then provided with a special emphasis on the contributions of GRC. With the increased emphasis on aircraft safety, enhanced performance, and affordability, as well as the need to reduce the environmental impact of aircraft, there are many new challenges being faced by the designers of aircraft propulsion systems. The Controls and Dynamics Branch (CDB) at the GRC is leading and participating in various projects to develop advanced propulsion controls and diagnostics technologies that will help meet the challenging goals of NASA Aeronautics Research Mission programs. The rest of the paper provides an overview of the various CDB technology development activities in aircraft engine control and diagnostics, both current and some accomplished in the recent past. The motivation for each of the research efforts, the research approach, technical challenges, and the key progress to date are summarized. DOI: 10.1061/(ASCE)AS.1943-5525.0000296. (C) 2013 American Society of Civil Engineers.
C1 NASA, Controls & Dynam Branch, Glenn Res Ctr, Cleveland, OH 44135 USA.
RP Garg, S (reprint author), NASA, Controls & Dynam Branch, Glenn Res Ctr, 21000 Brookpk Rd, Cleveland, OH 44135 USA.
EM sanjay.garg@nasa.gov
NR 47
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U1 2
U2 28
PU ASCE-AMER SOC CIVIL ENGINEERS
PI RESTON
PA 1801 ALEXANDER BELL DR, RESTON, VA 20191-4400 USA
SN 0893-1321
J9 J AEROSPACE ENG
JI J. Aerosp. Eng.
PD APR
PY 2013
VL 26
IS 2
SI SI
BP 422
EP 438
DI 10.1061/(ASCE)AS.1943-5525.0000296
PG 17
WC Engineering, Aerospace; Engineering, Civil
SC Engineering
GA 118YR
UT WOS:000317063900018
ER
PT J
AU Sharp, LM
Dietrich, DL
Motil, BJ
AF Sharp, Lauren M.
Dietrich, Daniel L.
Motil, Brian J.
TI Microgravity Fluids and Combustion Research at NASA Glenn Research
Center
SO JOURNAL OF AEROSPACE ENGINEERING
LA English
DT Article
DE Microgravity; Fluid physics; Combustion science
ID JET DIFFUSION FLAMES; REDUCED GRAVITY; BEHAVIOR; SPREAD
AB At the dawn of the Space Age, the design of early rocket and spacecraft systems presented significant challenges because of the low-gravity environment of space. Motivated by these challenges, the National Aeronautics and Space Administration (NASA) Glenn Research Center (GRC) pioneered the development of low-gravity facilities-including drop towers, sounding rockets, zero-gravity (zero-g) aircraft, and most importantly, space-based facilities-to advance microgravity research to further the nation's space exploration efforts. These efforts resulted in improved spacecraft system designs and practices in areas as diverse as fluid handling and spacecraft fire safety. At the same time, researchers realized that the microgravity environment allows the study of fundamental combustion and fluid physics problems, without the complication of buoyancy-induced convection. Microgravity testing enabled advancements in areas of technological and ecological importance in terrestrial applications such as global atmospheric change, combustor design, groundwater pollution, oil production, and advanced materials manufacturing, which often rely on advances in fluid physics and chemically reacting flows. GRC has been a leader in microgravity fluid physics and combustion research for more than 50 years. This paper highlights the facilities and some of the many accomplishments. DOI: 10.1061/(ASCE)AS.1943-5525.0000293. (C) 2013 American Society of Civil Engineers.
C1 [Sharp, Lauren M.; Dietrich, Daniel L.] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA.
[Motil, Brian J.] NASA, Fluid Phys & Transport Branch, Glenn Res Ctr, Cleveland, OH 44135 USA.
RP Sharp, LM (reprint author), NASA, Glenn Res Ctr, 21000 Brookpk Rd, Cleveland, OH 44135 USA.
EM Lauren.M.Sharp@nasa.gov; Daniel.L.Dietrich@nasa.gov;
Brian.J.Motil@nasa.gov
NR 34
TC 0
Z9 1
U1 3
U2 23
PU ASCE-AMER SOC CIVIL ENGINEERS
PI RESTON
PA 1801 ALEXANDER BELL DR, RESTON, VA 20191-4400 USA
SN 0893-1321
J9 J AEROSPACE ENG
JI J. Aerosp. Eng.
PD APR
PY 2013
VL 26
IS 2
SI SI
BP 439
EP 450
DI 10.1061/(ASCE)AS.1943-5525.0000293
PG 12
WC Engineering, Aerospace; Engineering, Civil
SC Engineering
GA 118YR
UT WOS:000317063900019
ER
PT J
AU Myers, J
Stauber, L
Weaver, A
McKay, T
Harrivel, A
Hepp, A
AF Myers, Jerry
Stauber, Laurel
Weaver, Aaron
McKay, Terri
Harrivel, Angela
Hepp, Aloysius
TI Bioscience and Medical Technology: From the Earth to Space and Back
SO JOURNAL OF AEROSPACE ENGINEERING
LA English
DT Article
DE Aerospace engineering; Aerospace medicine; Bioengineering; Biosciences;
Computer models; Community relations; Data communication; Data analysis;
Space exploration; Space life support systems
ID NANOTUBES; FORCES; CARBON
AB Throughout the 70-year history of NASA Glenn Research Center (GRC), technology development efforts that promoted advancement in aeronautics technologies, aerospace sciences, materials for hostile environments, and microgravity physics have also enabled the maturation of technologies that have affected medical practice on Earth, in the air, and in space. GRC's unique skill mix, required for aeronautics research and space exploration, ultimately also advanced the development of a wide array of capabilities applicable to biomedical engineering. This paper presents a historical review of notable biomedical endeavors at GRC that have addressed common and uncommon medical conditions afflicting both astronauts and non-astronauts. It also highlights the unique physiological stressors associated with residing in space. The physiological changes associated with these stimuli present evolving challenges for researchers to devise new and innovative medical interventions and technologies. DOI: 10.1061/(ASCE)AS.1943-5525.0000279. (C) 2013 American Society of Civil Engineers.
C1 [Myers, Jerry] NASA, Bio Sci & Technol Branch, Glenn Res Ctr, Cleveland, OH 44135 USA.
[Stauber, Laurel] NASA, Technol Collaborat, Glenn Res Ctr, Cleveland, OH 44135 USA.
[Weaver, Aaron; McKay, Terri; Harrivel, Angela; Hepp, Aloysius] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA.
RP Myers, J (reprint author), NASA, Bio Sci & Technol Branch, Glenn Res Ctr, Cleveland, OH 44135 USA.
EM jerry.g.myers@nasa.gov
NR 48
TC 0
Z9 0
U1 3
U2 15
PU ASCE-AMER SOC CIVIL ENGINEERS
PI RESTON
PA 1801 ALEXANDER BELL DR, RESTON, VA 20191-4400 USA
SN 0893-1321
J9 J AEROSPACE ENG
JI J. Aerosp. Eng.
PD APR
PY 2013
VL 26
IS 2
SI SI
BP 451
EP 458
DI 10.1061/(ASCE)AS.1943-5525.0000279
PG 8
WC Engineering, Aerospace; Engineering, Civil
SC Engineering
GA 118YR
UT WOS:000317063900020
ER
PT J
AU Misra, AK
Greenbauer-Seng, LA
AF Misra, Ajay K.
Greenbauer-Seng, Leslie A.
TI Aerospace Propulsion and Power Materials and Structures Research at NASA
Glenn Research Center
SO JOURNAL OF AEROSPACE ENGINEERING
LA English
DT Article
DE High-temperature materials and structures; Composite materials; Smart
materials; Nanomaterials; Impact dynamics; Active structures; Rotating
and dynamic structures; Multiscale modeling; Energy storage; Composite
mechanics
ID POLYMER MATRIX COMPOSITES; MECHANICAL-PROPERTIES; PROGRESSIVE DAMAGE;
BARRIER COATINGS; SILICON-CARBIDE; BEHAVIOR; PERFORMANCE; OXIDATION;
POLYIMIDE; CERAMICS
AB The National Aeronautics and Space Administration (NASA) Glenn Research Center (GRC) is well recognized for its contributions toward development of advanced materials and structures for aerospace propulsion and power systems. The Structures and Materials Division conducts research across a broad range of technical areas relevant to the agency's future aeronautics and space mission requirements. This paper will introduce the technical areas of strategic importance in the Structures and Materials Division today and briefly address some of the specific research activities within these areas. A broad look at how the research areas of emphasis have evolved over time, beginning in the early 1940s when the GRC was first formed, will be discussed. Examples of some of the more notable research accomplishments and their impact on the aerospace industry over this time period will be included. A discussion of the division's planned technical directions believed to be required to meet the longer-term national aeronautics and space exploration goals will also be addressed. DOI: 10.1061/(ASCE)AS.1943-5525.0000325. (C) 2013 American Society of Civil Engineers.
C1 [Misra, Ajay K.; Greenbauer-Seng, Leslie A.] NASA, Struct & Mat Div, Glenn Res Ctr, Cleveland, OH 44135 USA.
RP Greenbauer-Seng, LA (reprint author), NASA, Struct & Mat Div, Glenn Res Ctr, 21000 Brookpk Rd, Cleveland, OH 44135 USA.
EM Ajay.K.Misra@nasa.gov; Leslie.A.Greenbauer-Seng@nasa.gov
NR 142
TC 2
Z9 2
U1 8
U2 31
PU ASCE-AMER SOC CIVIL ENGINEERS
PI RESTON
PA 1801 ALEXANDER BELL DR, RESTON, VA 20191-4400 USA
SN 0893-1321
J9 J AEROSPACE ENG
JI J. Aerosp. Eng.
PD APR
PY 2013
VL 26
IS 2
SI SI
BP 459
EP 490
DI 10.1061/(ASCE)AS.1943-5525.0000325
PG 32
WC Engineering, Aerospace; Engineering, Civil
SC Engineering
GA 118YR
UT WOS:000317063900021
ER
PT J
AU Nathal, MV
Stefko, GL
AF Nathal, Michael V.
Stefko, George L.
TI Smart Materials and Active Structures
SO JOURNAL OF AEROSPACE ENGINEERING
LA English
DT Article
DE Shape memory alloys; Morphing structures; Forced vibration response
analysis; High-temperature piezoelectric materials; Rotating blade
vibration damping; Shunted piezoelectric damping; Blade spin rig;
Composite materials; Fan blade
ID MORPHOTROPIC PHASE-BOUNDARY; CERAMICS; NITI
AB Research in smart materials and active structures has grown significantly at the National Aeronautics and Space Administration (NASA) Glenn Research Center (GRC) in the last 10 years. The GRC has achieved several promising results in both new material development and component applications for concepts using both shape memory alloys and piezoelectric ceramics. Progress in understanding and modeling of shape memory alloys has allowed for improved design and control methodologies. New high-temperature alloys with attractive work output have extended the capability from room temperature to similar to 350 degrees C. Finally, the list of successful prototype demonstrations continues to grow for both commercially available alloys and the newer high-temperature alloys. Analytical and experimental methods on piezoelectric blade vibration damping have produced the first successful demonstration of vibration damping on a rotating component. The damping levels achieved lead to reduced dynamic stresses, hence increased engine life and enhanced damage tolerance. In addition, new compositions have been developed to extend the temperature capability of high-performance piezoelectrics to near 400 degrees C. These new materials are just now showing laboratory-scale feasibility and are targeted for continued development. DOI: 10.1061/(ASCE)AS.1943-5525.0000319. (C) 2013 American Society of Civil Engineers.
C1 [Nathal, Michael V.] NASA, Adv Metall Branch, Glenn Res Ctr, Cleveland, OH 44135 USA.
[Stefko, George L.] NASA, Struct & Dynam Branch, Glenn Res Ctr, Cleveland, OH 44135 USA.
RP Nathal, MV (reprint author), NASA, Adv Metall Branch, Glenn Res Ctr, 21000 Brookpk Rd, Cleveland, OH 44135 USA.
EM michael.v.nathal@nasa.gov; george.l.stefko@nasa.gov
FU NASA; Air Force Office of Scientific Research [FA9550-06-1-0260]
FX The work presented in this paper was the result of the efforts of the
following researchers: M. A. Bakhle, B. B. Choi, K. P. Duffy, J. B. Min,
C. R. Morrison, and A. J. Provenza (piezoelectric damping team); F.
Dynys, A. Sayir, and A. Sehirlioglu (high-temperature piezoelectric
material team); and G. S. Bigelow, O. Benafan, A. Garg, D. J. Gaydosh,
R. D. Noebe, and S. A. Padula (shape memory alloy team). Funding from
NASA's Subsonics Fixed Wing and Supersonics projects and Air Force
Office of Scientific Research Grant No. FA9550-06-1-0260 is appreciated.
NR 31
TC 1
Z9 1
U1 4
U2 85
PU ASCE-AMER SOC CIVIL ENGINEERS
PI RESTON
PA 1801 ALEXANDER BELL DR, RESTON, VA 20191-4400 USA
SN 0893-1321
J9 J AEROSPACE ENG
JI J. Aerosp. Eng.
PD APR
PY 2013
VL 26
IS 2
SI SI
BP 491
EP 499
DI 10.1061/(ASCE)AS.1943-5525.0000319
PG 9
WC Engineering, Aerospace; Engineering, Civil
SC Engineering
GA 118YR
UT WOS:000317063900022
ER
PT J
AU Dever, JA
Nathal, MV
DiCarlo, JA
AF Dever, Joyce A.
Nathal, Michael V.
DiCarlo, James A.
TI Research on High-Temperature Aerospace Materials at NASA Glenn Research
Center
SO JOURNAL OF AEROSPACE ENGINEERING
LA English
DT Article
DE Metallic materials; Ceramic materials; Ceramic matrix composites;
Thermal barrier coatings; Environmental barrier coatings; Oxidation; Hot
corrosion
ID THERMAL BARRIER COATINGS; SIO2 SCALE VOLATILITY; CYCLIC-OXIDATION
BEHAVIOR; SILICON-CARBIDE; THERMOMECHANICAL PROPERTIES; COMBUSTION
CONDITIONS; MATRIX COMPOSITES; SIC FIBERS; CERAMICS; MODEL
AB Within the Structures and Materials Division at the National Aeronautics and Space Administration Glenn Research Center (GRC), research is being conducted to develop durable high-temperature materials for the most challenging aerospace applications. Research is advancing material and coating technologies for applications including turbine engine hot section components, rocket engine combustion chamber liners, high-temperature components of advanced space power systems, and atmospheric reentry vehicle surfaces. As part of the volume of papers recognizing 70 years of research at the GRC, this paper summarizes key research contributions that GRC has made to the field of high-temperature aerospace materials. DOI: 10.1061/(ASCE)AS.1943-5525.0000321. (C) 2013 American Society of Civil Engineers.
C1 [Dever, Joyce A.] NASA, Durabil & Protect Coatings Branch, Glenn Res Ctr, Cleveland, OH 44135 USA.
[Nathal, Michael V.] NASA, Adv Metall Branch, Glenn Res Ctr, Cleveland, OH 44135 USA.
[DiCarlo, James A.] NASA, Struct & Mat Div, Glenn Res Ctr, Cleveland, OH 44135 USA.
RP Dever, JA (reprint author), NASA, Durabil & Protect Coatings Branch, Glenn Res Ctr, 21000 Brookpk Rd, Cleveland, OH 44135 USA.
EM Joyce.A.Dever@nasa.gov; Michael.V.Nathal@nasa.gov;
James.A.DiCarlo@nasa.gov
NR 102
TC 4
Z9 5
U1 2
U2 61
PU ASCE-AMER SOC CIVIL ENGINEERS
PI RESTON
PA 1801 ALEXANDER BELL DR, RESTON, VA 20191-4400 USA
SN 0893-1321
J9 J AEROSPACE ENG
JI J. Aerosp. Eng.
PD APR
PY 2013
VL 26
IS 2
SI SI
BP 500
EP 514
DI 10.1061/(ASCE)AS.1943-5525.0000321
PG 15
WC Engineering, Aerospace; Engineering, Civil
SC Engineering
GA 118YR
UT WOS:000317063900023
ER
PT J
AU Kaufman, I
Luchinsky, DG
Tindjong, R
McClintock, PVE
Eisenberg, RS
AF Kaufman, I.
Luchinsky, D. G.
Tindjong, R.
McClintock, P. V. E.
Eisenberg, R. S.
TI Multi-ion conduction bands in a simple model of calcium ion channels
SO PHYSICAL BIOLOGY
LA English
DT Article
ID GATED SODIUM-CHANNEL; SELECTIVITY; PERMEATION; MECHANISM; SIMULATION;
MUTATIONS; MEMBRANE
AB We report self-consistent Brownian dynamics simulations of a simple electrostatic model of the selectivity filters (SF) of calcium ion channels. They reveal regular structure in the conductance and selectivity as functions of the fixed negative charge Q(f) at the SF. With increasing Q(f), there are distinct regions of high conductance (conduction bands) M0, M1, M2 separated by regions of almost zero-conductance (stop-bands). Two of these conduction bands, M1 and M2, are related to the saturated calcium occupancies of P = 1 and P = 2, respectively and demonstrate self-sustained conductivity. Despite the model's limitations, its M1 and M2 bands show high calcium selectivity and prominent anomalous mole fraction effects and can be identified with the L-type and RyR calcium channels. The non-selective band M0 can be identified with a non-selective cation channel, or with OmpF porin.
C1 [Kaufman, I.; Luchinsky, D. G.; Tindjong, R.; McClintock, P. V. E.] Univ Lancaster, Dept Phys, Lancaster LA1 4YB, England.
[Luchinsky, D. G.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Eisenberg, R. S.] Rush Med Coll, Dept Physiol & Mol Biophys, Chicago, IL 60612 USA.
RP Kaufman, I (reprint author), Univ Lancaster, Dept Phys, Lancaster LA1 4YB, England.
EM p.v.e.mcclintock@lancaster.ac.uk
FU Engineering and Physical Sciences Research Council (EPSRC)
[EP/G070660/1]
FX This work was supported by Engineering and Physical Sciences Research
Council (EPSRC) (grant no EP/G070660/1).
NR 36
TC 12
Z9 12
U1 1
U2 17
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 1478-3967
EI 1478-3975
J9 PHYS BIOL
JI Phys. Biol.
PD APR
PY 2013
VL 10
IS 2
AR 026007
DI 10.1088/1478-3975/10/2/026007
PG 8
WC Biochemistry & Molecular Biology; Biophysics
SC Biochemistry & Molecular Biology; Biophysics
GA 119NE
UT WOS:000317103500013
PM 23481350
ER
PT J
AU Cutler, AD
Harding, GC
Diskin, GS
AF Cutler, A. D.
Harding, G. C.
Diskin, G. S.
TI High Frequency Pulsed Injection into a Supersonic Duct Flow
SO AIAA JOURNAL
LA English
DT Article
ID CROSS-FLOW; JETS; PENETRATION
AB A study is presented of the effect of pulsation (100% modulation) of a sonic jet of helium into a supersonic (ducted) crossflow on its mixing. An injector was developed to provide a high-speed high-frequency (up to 13 kHz) pulsed jet. The injector nozzle is formed between fixed internal passages and a three- or four-sided wheel embedded within the device that rotates due to the flow in the nozzle. For a given geometry the pulsation frequency is repeatable, constant above a certain pressure ratio, and scales with the speed of sound of the gas. The pulsed jet in the crossflow was visualized in a side view by schlieren photography. The plume of injected helium was visualized in a cross section, 69 effective jet diameters downstream of injection, by seeding the helium with a small amount of ethanol, which condensed as tiny particles and illuminated with a laser light sheet. Results indicate a modest reduction in mean plume cross-sectional size (and, therefore, reduction of mixing) with pulsation and an increase in mean helium penetration. The visualization results are consistent with a transitional state between the turbulent puffs and vortex rings previously observed in low-speed experiments on subsonic pulsed jets in crossflow.
C1 [Cutler, A. D.; Harding, G. C.] George Washington Univ, Newport News, VA 23602 USA.
[Diskin, G. S.] NASA, Langley Res Ctr, Hampton, VA 23681 USA.
RP Cutler, AD (reprint author), George Washington Univ, Newport News, VA 23602 USA.
NR 27
TC 2
Z9 2
U1 1
U2 18
PU AMER INST AERONAUTICS ASTRONAUTICS
PI RESTON
PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA
SN 0001-1452
EI 1533-385X
J9 AIAA J
JI AIAA J.
PD APR
PY 2013
VL 51
IS 4
BP 809
EP 818
DI 10.2514/1.J051620
PG 10
WC Engineering, Aerospace
SC Engineering
GA 115QP
UT WOS:000316827300005
ER
PT J
AU Erkmen, BI
Barber, ZW
Dahl, J
AF Erkmen, Baris I.
Barber, Zeb W.
Dahl, Jason
TI Maximum-likelihood estimation for frequency-modulated continuous-wave
laser ranging using photon-counting detectors
SO APPLIED OPTICS
LA English
DT Article
ID HETERODYNE-DETECTION; PERFORMANCE; RADAR; LADAR
AB We analyze the minimum achievable mean-square error in frequency-modulated continuous-wave range estimation of a single stationary target when photon-counting detectors are employed. Starting from the probability density function for the photon-arrival times in photodetectors with subunity quantum efficiency, dark counts, and dead time, we derive the Cramer-Rao bound and highlight three important asymptotic regimes. We then derive the maximum-likelihood (ML) estimator for arbitrary frequency modulation. Simulation of the ML estimator shows that its performance approaches the standard quantum limit only when the mean received photons are between two thresholds. We provide analytic approximations to these thresholds for linear frequency modulation. We also compare the ML estimator's performance to conventional Fourier transform (FT) frequency estimation, showing that they are equivalent if the reference arm is much stronger than the target return, but that when the reference field is weak the FT estimator is suboptimal by approximately a factor of root 2 in root-mean-square error. Finally, we report on a proof-of-concept experiment in which the ML estimator achieves this theoretically predicted improvement over the FT estimator. (C) 2013 Optical Society of America
C1 [Erkmen, Baris I.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Barber, Zeb W.; Dahl, Jason] Montana State Univ, Spectrum Lab, Bozeman, MT 59717 USA.
RP Erkmen, BI (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM baris.i.erkmen@jpl.nasa.gov
FU DARPA InPho [PROP. 81-17433]; National Aeronautics and Space
Administration; DARPA InPho, Army Research Office [W911NF-11-1-0540]
FX The authors thank the anonymous reviewers for their detailed feedback,
which has greatly improved the manuscript. BIE's contributions to the
research described in this paper were supported by the DARPA InPho,
contract PROP. 81-17433, and were carried out by the Jet Propulsion
Laboratory, California Institute of Technology, under a contract with
the National Aeronautics and Space Administration. ZWB's and JD's
contributions were supported by DARPA InPho, Army Research Office Grant
W911NF-11-1-0540.
NR 21
TC 1
Z9 1
U1 1
U2 8
PU OPTICAL SOC AMER
PI WASHINGTON
PA 2010 MASSACHUSETTS AVE NW, WASHINGTON, DC 20036 USA
SN 1559-128X
EI 2155-3165
J9 APPL OPTICS
JI Appl. Optics
PD APR 1
PY 2013
VL 52
IS 10
BP 2008
EP 2018
DI 10.1364/AO.52.002008
PG 11
WC Optics
SC Optics
GA 117YB
UT WOS:000316988100016
PM 23545955
ER
PT J
AU Werdell, PJ
Franz, BA
Bailey, SW
Feldman, GC
Boss, E
Brando, VE
Dowell, M
Hirata, T
Lavender, SJ
Lee, ZP
Loisel, H
Maritorena, S
Melin, F
Moore, TS
Smyth, TJ
Antoine, D
Devred, E
d'Andon, OHF
Mangin, A
AF Werdell, P. Jeremy
Franz, Bryan A.
Bailey, Sean W.
Feldman, Gene C.
Boss, Emmanuel
Brando, Vittorio E.
Dowell, Mark
Hirata, Takafumi
Lavender, Samantha J.
Lee, ZhongPing
Loisel, Hubert
Maritorena, Stephane
Melin, Frederic
Moore, Timothy S.
Smyth, Timothy J.
Antoine, David
Devred, Emmanuel
d'Andon, Odile Hembise Fanton
Mangin, Antoine
TI Generalized ocean color inversion model for retrieving marine inherent
optical properties
SO APPLIED OPTICS
LA English
DT Article
ID WATER-LEAVING RADIANCES; PHYTOPLANKTON ABSORPTION; CHLOROPHYLL-A;
SEMIANALYTICAL MODEL; LIGHT ATTENUATION; BIOOPTICAL MODEL; COASTAL
WATERS; CHESAPEAKE BAY; DATA PRODUCTS; TIME-SERIES
AB Ocean color measured from satellites provides daily, global estimates of marine inherent optical properties (IOPs). Semi-analytical algorithms (SAAs) provide one mechanism for inverting the color of the water observed by the satellite into IOPs. While numerous SAAs exist, most are similarly constructed and few are appropriately parameterized for all water masses for all seasons. To initiate community-wide discussion of these limitations, NASA organized two workshops that deconstructed SAAs to identify similarities and uniqueness and to progress toward consensus on a unified SAA. This effort resulted in the development of the generalized IOP (GIOP) model software that allows for the construction of different SAAs at runtime by selection from an assortment of model parameterizations. As such, GIOP permits isolation and evaluation of specific modeling assumptions, construction of SAAs, development of regionally tuned SAAs, and execution of ensemble inversion modeling. Working groups associated with the workshops proposed a preliminary default configuration for GIOP (GIOP-DC), with alternative model parameterizations and features defined for subsequent evaluation. In this paper, we: (1) describe the theoretical basis of GIOP; (2) present GIOP-DC and verify its comparable performance to other popular SAAs using both in situ and synthetic data sets; and, (3) quantify the sensitivities of their output to their parameterization. We use the latter to develop a hierarchical sensitivity of SAAs to various model parameterizations, to identify components of SAAs that merit focus in future research, and to provide material for discussion on algorithm uncertainties and future emsemble applications. (C) 2013 Optical Society of America
C1 [Werdell, P. Jeremy; Franz, Bryan A.; Bailey, Sean W.; Feldman, Gene C.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Werdell, P. Jeremy; Boss, Emmanuel] Univ Maine, Sch Marine Sci, Orono, ME 04401 USA.
[Bailey, Sean W.] Futuretech Corp, Greenbelt, MD 20770 USA.
[Brando, Vittorio E.] CSIRO Land & Water, Environm Earth Observat Program, Canberra, ACT, Australia.
[Dowell, Mark; Melin, Frederic] Commiss European Communities, Joint Res Ctr, I-21027 Ispra, Italy.
[Hirata, Takafumi] Hokkaido Univ, Fac Environm Earth Sci, Sapporo, Hokkaido 0600810, Japan.
[Lavender, Samantha J.] Pixalytics Ltd, Plymouth PL6 8BX, Devon, England.
[Lee, ZhongPing] Univ Massachusetts, Boston, MA 02125 USA.
[Loisel, Hubert] Univ Littoral Cote dOpale, Lab Oceanol & Geosci, F-62930 Wimereux, France.
[Maritorena, Stephane] Univ Calif Santa Barbara, Earth Res Inst, Santa Barbara, CA 93106 USA.
[Moore, Timothy S.] Univ New Hampshire, Ocean Proc Anal Lab, Durham, NH 03824 USA.
[Smyth, Timothy J.] Plymouth Marine Lab, Plymouth PL1 3DH, Devon, England.
[Antoine, David] CNRS, Lab Oceanog Villefranche, F-06238 Villefranche Sur Mer, France.
[Devred, Emmanuel] Univ Laval, Joint Int Lab, Unite Mixte Int Takuv, Quebec City, PQ GV1 0AG, Canada.
[d'Andon, Odile Hembise Fanton; Mangin, Antoine] ACRI ST, F-06904 Sophia Antipolis, France.
RP Werdell, PJ (reprint author), NASA, Goddard Space Flight Ctr, Code 616, Greenbelt, MD 20771 USA.
EM jeremy.werdell@nasa.gov
RI Antoine, David/C-3817-2013; Werdell, Jeremy/D-8265-2012; Boss,
Emmanuel/C-5765-2009; Franz, Bryan/D-6284-2012; Brando,
Vittorio/A-1321-2008; Hirata, Takafumi/F-7854-2012; Bailey,
Sean/D-3077-2017
OI Antoine, David/0000-0002-9082-2395; Boss, Emmanuel/0000-0002-8334-9595;
Franz, Bryan/0000-0003-0293-2082; Brando, Vittorio/0000-0002-2193-5695;
Hirata, Takafumi/0000-0003-1258-1837; Bailey, Sean/0000-0001-8339-9763
FU NASA MODIS Science Team; CSIRO Wealth from Oceans Flagship
FX We thank Mike Behrenfeld, Paula Bontempi, Catherine Brown, Yannick Huot,
Paul Lyon, Constant Mazeran, and Jill Schwarz for their helpful advice
and participation in the NASA GIOP workshops. We also thank an anonymous
reviewer for useful comments that improved this manuscript. Support for
this work was provided through the NASA MODIS Science Team (P.J.W., B.
A. F., S. W. B.) and the CSIRO Wealth from Oceans Flagship (V.B.).
NR 60
TC 51
Z9 52
U1 7
U2 49
PU OPTICAL SOC AMER
PI WASHINGTON
PA 2010 MASSACHUSETTS AVE NW, WASHINGTON, DC 20036 USA
SN 1559-128X
EI 2155-3165
J9 APPL OPTICS
JI Appl. Optics
PD APR 1
PY 2013
VL 52
IS 10
BP 2019
EP 2037
DI 10.1364/AO.52.002019
PG 19
WC Optics
SC Optics
GA 117YB
UT WOS:000316988100017
PM 23545956
ER
PT J
AU Chaplin, WJ
Sanchis-Ojeda, R
Campante, TL
Handberg, R
Stello, D
Winn, JN
Basu, S
Christensen-Dalsgaard, J
Davies, GR
Metcalfe, TS
Buchhave, LA
Fischer, DA
Bedding, TR
Cochran, WD
Elsworth, Y
Gilliland, RL
Hekker, S
Huber, D
Isaacson, H
Karoff, C
Kawaler, SD
Kjeldsen, H
Latham, DW
Lund, MN
Lundkvist, M
Marcy, GW
Miglio, A
Barclay, T
Lissauer, JJ
AF Chaplin, W. J.
Sanchis-Ojeda, R.
Campante, T. L.
Handberg, R.
Stello, D.
Winn, J. N.
Basu, S.
Christensen-Dalsgaard, J.
Davies, G. R.
Metcalfe, T. S.
Buchhave, L. A.
Fischer, D. A.
Bedding, T. R.
Cochran, W. D.
Elsworth, Y.
Gilliland, R. L.
Hekker, S.
Huber, D.
Isaacson, H.
Karoff, C.
Kawaler, S. D.
Kjeldsen, H.
Latham, D. W.
Lund, M. N.
Lundkvist, M.
Marcy, G. W.
Miglio, A.
Barclay, T.
Lissauer, J. J.
TI ASTEROSEISMIC DETERMINATION OF OBLIQUITIES OF THE EXOPLANET SYSTEMS
KEPLER-50 AND KEPLER-65
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE asteroseismology; planets and satellites: formation; planets and
satellites: general; stars: rotation
ID SPIN-ORBIT MISALIGNMENT; SOLAR-TYPE STARS; TRANSIT TIMING OBSERVATIONS;
RAPIDLY ROTATING STARS; OF-STATE TABLES; SUN-LIKE STAR; PLANET
CANDIDATES; LIGHT CURVES; PHOTOMETRIC VARIABILITY; INITIAL
CHARACTERISTICS
AB Results on the obliquity of exoplanet host stars-the angle between the stellar spin axis and the planetary orbital axis-provide important diagnostic information for theories describing planetary formation. Here we present the first application of asteroseismology to the problem of stellar obliquity determination in systems with transiting planets and Sun-like host stars. We consider two systems observed by the NASA Kepler mission which have multiple transiting small (super-Earth sized) planets: the previously reported Kepler-50 and a new system, Kepler-65, whose planets we validate in this paper. Both stars show rich spectra of solar-like oscillations. From the asteroseismic analysis we find that each host has its rotation axis nearly perpendicular to the line of sight with the sines of the angles constrained at the 1 sigma level to lie above 0.97 and 0.91, respectively. We use statistical arguments to show that coplanar orbits are favored in both systems, and that the orientations of the planetary orbits and the stellar rotation axis are correlated.
C1 [Chaplin, W. J.; Campante, T. L.; Davies, G. R.; Elsworth, Y.; Hekker, S.; Miglio, A.] Univ Birmingham, Sch Phys & Astron, Birmingham B15 2TT, W Midlands, England.
[Sanchis-Ojeda, R.; Winn, J. N.] MIT, Dept Phys, Cambridge, MA 02139 USA.
[Handberg, R.; Christensen-Dalsgaard, J.; Karoff, C.; Kjeldsen, H.; Lund, M. N.; Lundkvist, M.] Aarhus Univ, Dept Phys & Astron, SAC, DK-8000 Aarhus C, Denmark.
[Stello, D.; Bedding, T. R.] Univ Sydney, Sch Phys, Sydney Inst Astron, Sydney, NSW 2006, Australia.
[Basu, S.; Fischer, D. A.] Yale Univ, New Haven, CT 06520 USA.
[Metcalfe, T. S.] White Dwarf Res Corp, Boulder, CO 80301 USA.
[Buchhave, L. A.] Univ Copenhagen, Niels Bohr Inst, DK-2100 Copenhagen, Denmark.
[Buchhave, L. A.] Univ Copenhagen, Nat Hist Museum Denmark, Ctr Star & Planet Format, DK-1530 Copenhagen, Denmark.
[Cochran, W. D.] Univ Texas Austin, McDonald Observ, Austin, TX 78712 USA.
[Gilliland, R. L.] Penn State Univ, Ctr Exoplanets & Habitable Worlds, University Pk, PA 16802 USA.
[Hekker, S.] Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1098 XH Amsterdam, Netherlands.
[Huber, D.; Barclay, T.; Lissauer, J. J.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Isaacson, H.; Marcy, G. W.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA.
[Kawaler, S. D.] Iowa State Univ, Dept Phys & Astron, Ames, IA 50011 USA.
[Latham, D. W.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Barclay, T.] Environm Res Inst, Bay Area, Sonoma, CA 95476 USA.
RP Chaplin, WJ (reprint author), Univ Birmingham, Sch Phys & Astron, Birmingham B15 2TT, W Midlands, England.
OI Kawaler, Steven/0000-0002-6536-6367; Bedding,
Timothy/0000-0001-5943-1460; Davies, Guy/0000-0002-4290-7351; Buchhave,
Lars A./0000-0003-1605-5666; Metcalfe, Travis/0000-0003-4034-0416;
Karoff, Christoffer/0000-0003-2009-7965; Bedding,
Tim/0000-0001-5222-4661; Basu, Sarbani/0000-0002-6163-3472; Lund, Mikkel
Norup/0000-0001-9214-5642; Lundkvist, Mia Sloth/0000-0002-8661-2571;
Fischer, Debra/0000-0003-2221-0861; Handberg, Rasmus/0000-0001-8725-4502
FU NASA's Science Mission Directorate; UK Science and Technology Facilities
Council (STFC); NASA Kepler Participating Scientist program
[NNX12AC76G]; NSF [AST 1105930]; Danish National Research Foundation;
ASTERISK project (ASTERoseismic Investigations with SONG and Kepler);
European Research Council [267864]; Netherlands Organisation for
Scientific Research (NWO); International Space Science Institute (ISSI)
FX Funding for this Discovery mission is provided by NASA's Science Mission
Directorate. The authors wish to thank the entire Kepler team, without
whom these results would not be possible. W.J.C., T.L.C., G.R. D., Y.E.,
and A. M. acknowledge the support of the UK Science and Technology
Facilities Council (STFC). J.N.W. was supported by the NASA Kepler
Participating Scientist program through grant NNX12AC76G. S.B.
acknowledges NSF grant AST 1105930. Funding for the Stellar Astrophysics
Centre (SAC) is provided by The Danish National Research Foundation. The
research is supported by the ASTERISK project (ASTERoseismic
Investigations with SONG and Kepler) funded by the European Research
Council (grant agreement no.:267864). S.H. acknowledges financial
support from the Netherlands Organisation for Scientific Research (NWO).
Computational time on Kraken at the National Institute of Computational
Sciences was provided through NSF TeraGrid allocation TG-AST090107. We
acknowledge the Pale Blue Dot Project, hosted by White Dwarf Research
Corporation (whitedwarf.org/palebluedot), and we are also grateful for
support from the International Space Science Institute (ISSI).
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PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD APR 1
PY 2013
VL 766
IS 2
AR 101
DI 10.1088/0004-637X/766/2/101
PG 19
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 108UE
UT WOS:000316320900035
ER
PT J
AU Filacchione, G
Capaccioni, F
Clark, RN
Nicholson, PD
Cruikshank, DP
Cuzzi, JN
Lunine, JI
Brown, RH
Cerroni, P
Tosi, F
Ciarniello, M
Buratti, BJ
Hedman, MM
Flamini, E
AF Filacchione, G.
Capaccioni, F.
Clark, R. N.
Nicholson, P. D.
Cruikshank, D. P.
Cuzzi, J. N.
Lunine, J. I.
Brown, R. H.
Cerroni, P.
Tosi, F.
Ciarniello, M.
Buratti, B. J.
Hedman, M. M.
Flamini, E.
TI THE RADIAL DISTRIBUTION OF WATER ICE AND CHROMOPHORES ACROSS SATURN'S
SYSTEM
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE planets and satellites: composition; planets and satellites: rings
ID CASSINI-VIMS; SURFACE-COMPOSITION; DARK MATERIAL; RINGS; SATELLITES;
SPECTRA; IAPETUS; ENCELADUS; PHOEBE; DISK
AB Over the past eight years, the Visual and Infrared Mapping Spectrometer (VIMS) on board the Cassini orbiter has returned hyperspectral images in the 0.35-5.1 mu m range of the icy satellites and rings of Saturn. These very different objects show significant variations in surface composition, roughness, and regolith grain size as a result of their evolutionary histories, endogenic processes, and interactions with exogenic particles. The distributions of surface water ice and chromophores, i.e., organic and non-icy materials, across the Saturnian system, are traced using specific spectral indicators (spectral slopes and absorption band depths) obtained from rings mosaics and disk-integrated satellites observations by VIMS. Moving from the inner C ring to Iapetus, we found a marking uniformity in the distribution of abundance of water ice. On the other hand, the distribution of chromophores is much more concentrated in the rings particles and on the outermost satellites (Rhea, Hyperion, and Iapetus). A reduction of red material is observed on the satellites' surfaces orbiting within the E ring environment likely due to fine particles from Enceladus' plumes. Once the exogenous dark material covering the Iapetus' leading hemisphere is removed, the texture of the water ice-rich surfaces, inferred through the 2 mu m band depth, appears remarkably uniform across the entire system.
C1 [Filacchione, G.; Capaccioni, F.; Cerroni, P.; Tosi, F.; Ciarniello, M.] Area Ric Tor Vergata, Ist Astrofis & Planetol Spaziali, INAF IAPS, I-00133 Rome, Italy.
[Clark, R. N.] US Geol Survey, Fed Ctr, Denver, CO 80228 USA.
[Nicholson, P. D.; Lunine, J. I.; Hedman, M. M.] Cornell Univ, Dept Astron, Ithaca, NY 14853 USA.
[Cruikshank, D. P.; Cuzzi, J. N.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Brown, R. H.] Univ Arizona, Lunar Planetary Lab, Tucson, AZ 85721 USA.
[Buratti, B. J.] CALTECH, NASA, Jet Prop Lab, Pasadena, CA 91109 USA.
[Flamini, E.] Italian Space Agcy, ASI, I-00198 Rome, Italy.
RP Filacchione, G (reprint author), Area Ric Tor Vergata, Ist Astrofis & Planetol Spaziali, INAF IAPS, Via Fosso Cavaliere 100, I-00133 Rome, Italy.
EM gianrico.filacchione@iaps.inaf.it
OI Ciarniello, Mauro/0000-0002-7498-5207; Cerroni,
Priscilla/0000-0003-0239-2741; Capaccioni, Fabrizio/0000-0003-1631-4314;
Filacchione, Gianrico/0000-0001-9567-0055; Tosi,
Federico/0000-0003-4002-2434
FU Italian Space Agency [I/015/09/0]; NASA through the Cassini project
FX This research has made use of NASA's Astrophysics Data System and was
completed thanks to the financial support of the Italian Space Agency
(grant I/015/09/0) and NASA through the Cassini project.
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PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD APR 1
PY 2013
VL 766
IS 2
AR 76
DI 10.1088/0004-637X/766/2/76
PG 5
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 108UE
UT WOS:000316320900010
ER
PT J
AU Fressin, F
Torres, G
Charbonneau, D
Bryson, ST
Christiansen, J
Dressing, CD
Jenkins, JM
Walkowicz, LM
Batalha, NM
AF Fressin, Francois
Torres, Guillermo
Charbonneau, David
Bryson, Stephen T.
Christiansen, Jessie
Dressing, Courtney D.
Jenkins, Jon M.
Walkowicz, Lucianne M.
Batalha, Natalie M.
TI THE FALSE POSITIVE RATE OF KEPLER AND THE OCCURRENCE OF PLANETS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE binaries: eclipsing; methods: data analysis; methods: statistical;
planetary systems
ID TRANSIT TIMING VARIATIONS; SOLAR-TYPE STARS; SUN-LIKE STARS; ECLIPSING
BINARIES; BLEND SCENARIOS; MULTIPLE SYSTEM; HABITABLE-ZONE; INPUT
CATALOG; DATA RELEASE; CANDIDATES
AB The Kepler mission is uniquely suited to study the frequencies of extrasolar planets. This goal requires knowledge of the incidence of false positives such as eclipsing binaries in the background of the targets, or physically bound to them, which can mimic the photometric signal of a transiting planet. We perform numerical simulations of the Kepler targets and of physical companions or stars in the background to predict the occurrence of astrophysical false positives detectable by the mission. Using real noise level estimates, we compute the number and characteristics of detectable eclipsing pairs involving main-sequence stars and non-main-sequence stars or planets, and we quantify the fraction of those that would pass the Kepler candidate vetting procedure. By comparing their distribution with that of the Kepler Objects of Interest (KOIs) detected during the first six quarters of operation of the spacecraft, we infer the false positive rate of Kepler and study its dependence on spectral type, candidate planet size, and orbital period. We find that the global false positive rate of Kepler is 9.4%, peaking for giant planets (6-22 R-circle plus) at 17.7%, reaching a low of 6.7% for small Neptunes (2-4 R-circle plus), and increasing again for Earth-size planets (0.8-1.25 R-circle plus) to 12.3%. Most importantly, we also quantify and characterize the distribution and rate of occurrence of planets down to Earth size with no prior assumptions on their frequency, by subtracting from the population of actual Kepler candidates our simulated population of astrophysical false positives. We find that 16.5% +/- 3.6% of main-sequence FGK stars have at least one planet between 0.8 and 1.25 R-circle plus with orbital periods up to 85 days. This result is a significant step toward the determination of eta-earth, the occurrence of Earth-like planets in the habitable zone of their parent stars. There is no significant dependence of the rates of planet occurrence between 0.8 and 4 Earth radii with spectral type. In the process, we also derive a prescription for the signal recovery rate of Kepler that enables a good match to both the KOI size and orbital period distribution, as well as their signal-to-noise distribution.
C1 [Fressin, Francois; Torres, Guillermo; Charbonneau, David; Dressing, Courtney D.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Bryson, Stephen T.; Christiansen, Jessie; Jenkins, Jon M.; Batalha, Natalie M.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Walkowicz, Lucianne M.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA.
RP Fressin, F (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
EM ffressin@cfa.harvard.edu
OI Charbonneau, David/0000-0002-9003-484X
FU NASA [NNX12AC75G]
FX We thank the anonymous referee for helpful suggestions on the original
manuscript. G.T. acknowledges partial support for this work from NASA
Grant NNX12AC75G (Kepler Participating Scientist Program).
NR 46
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PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD APR 1
PY 2013
VL 766
IS 2
AR 81
DI 10.1088/0004-637X/766/2/81
PG 20
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 108UE
UT WOS:000316320900015
ER
PT J
AU Hunana, P
Goldstein, ML
Passot, T
Sulem, PL
Laveder, D
Zank, GP
AF Hunana, P.
Goldstein, M. L.
Passot, T.
Sulem, P. L.
Laveder, D.
Zank, G. P.
TI POLARIZATION AND COMPRESSIBILITY OF OBLIQUE KINETIC ALFVEN WAVES
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE magnetohydrodynamics (MHD); solar wind; turbulence; waves
ID WEAKLY COLLISIONAL PLASMAS; LOW-FREQUENCY WAVES; SOLAR-WIND;
MAGNETOHYDRODYNAMIC TURBULENCE; ASTROPHYSICAL GYROKINETICS; HALL-MHD;
FLUID; MODEL; FLUCTUATIONS; EQUATIONS
AB It is well known that a complete description of the solar wind requires a kinetic description and that, particularly at sub-proton scales, kinetic effects cannot be ignored. It is nevertheless usually assumed that at scales significantly larger than the proton gyroscale r(L), magnetohydrodynamics or its extensions, such as Hall-MHD and two-fluid models with isotropic pressures, provide a satisfactory description of the solar wind. Here we calculate the polarization and magnetic compressibility of oblique kinetic Alfven waves and show that, compared with linear kinetic theory, the isotropic two-fluid description is very compressible, with the largest discrepancy occurring at scales larger than the proton gyroscale. In contrast, introducing anisotropic pressure fluctuations with the usual double-adiabatic (or CGL) equations of state yields compressibility values which are unrealistically low. We also show that both of these classes of fluid models incorrectly describe the electric field polarization. To incorporate linear kinetic effects, we use two versions of the Landau fluid model that include linear Landau damping and finite Larmor radius (FLR) corrections. We show that Landau damping is crucial for correct modeling of magnetic compressibility, and that the anisotropy of pressure fluctuations should not be introduced without taking into account the Landau damping through appropriate heat flux equations. We also show that FLR corrections to all the retained fluid moments appear to be necessary to yield the correct polarization. We conclude that kinetic effects cannot be ignored even for kr(L) << 1.
C1 [Hunana, P.; Goldstein, M. L.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Passot, T.; Sulem, P. L.; Laveder, D.] Univ Nice Sophia Antipolis, CNRS, Lab JL Lagrange, Observ Cote Azur, F-06304 Nice 4, France.
[Zank, G. P.] Univ Alabama, CSPAR, Huntsville, AL 35805 USA.
[Zank, G. P.] Univ Alabama, Dept Phys, Huntsville, AL 35899 USA.
RP Hunana, P (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RI NASA MMS, Science Team/J-5393-2013
OI NASA MMS, Science Team/0000-0002-9504-5214
FU Magnetospheric Multiscale mission at the Goddard Space Flight Center;
European Commission's Seventh Framework Programme [284515]; INSU-CNRS
"Programme Soleil-Terre"; NASA [NNX08AJ33G, Subaward 37102-2,
NNX09AG70G, NNX09AG63G, NNX09AJ79G, NNG05EC85C, Subcontract A991132BT,
NNX09AP74A]
FX P.H. was supported by NASA Postdoctoral Program, which is administered
by Oak Ridge Associated Universities (ORAU). M.L.G. was supported, in
part, by the Interdisciplinary Science program of the Magnetospheric
Multiscale mission at the Goddard Space Flight Center. The research
leading to these results has received funding from the European
Commission's Seventh Framework Programme (FP7/2007-2013) under the grant
agreement SHOCK (Project No. 284515). The support of INSU-CNRS
"Programme Soleil-Terre" is also acknowledged. We acknowledge the
partial support of NASA grants NNX08AJ33G, Subaward 37102-2, NNX09AG70G,
NNX09AG63G, NNX09AJ79G, NNG05EC85C, Subcontract A991132BT, NNX09AP74A,
NNX10AE46G, NNX09AW45G, and NSF grant ATM-0904007.
NR 45
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PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD APR 1
PY 2013
VL 766
IS 2
AR 93
DI 10.1088/0004-637X/766/2/93
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 108UE
UT WOS:000316320900027
ER
PT J
AU Paganini, L
Mumma, MJ
Boehnhardt, H
DiSanti, MA
Villanueva, GL
Bonev, BP
Lippi, M
Kaufl, HU
Blake, GA
AF Paganini, Lucas
Mumma, Michael J.
Boehnhardt, Hermann
DiSanti, Michael A.
Villanueva, Geronimo L.
Bonev, Boncho P.
Lippi, Manuela
Kaeufl, Hans U.
Blake, Geoffrey A.
TI GROUND-BASED INFRARED DETECTIONS OF CO IN THE CENTAUR-COMET
29P/SCHWASSMANN-WACHMANN 1 AT 6.26 AU FROM THE SUN
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE astrochemistry; comets: general; comets: individual
(29P/Schwassmann-Wachmann 1); Kuiper belt: general; molecular processes;
planets and satellites: formation
ID JUPITER-FAMILY COMETS; KUIPER-BELT OBJECTS; C/2009 P1 GARRADD; O1
HALE-BOPP; CARBON-MONOXIDE; CHEMICAL-COMPOSITION; OUTBURST ACTIVITY;
MODEL; BAND; ATMOSPHERES
AB We observed Comet 29P/Schwassmann-Wachmann 1 (hereafter, 29P) in 2012 February and May with CRIRES/VLT and NIRSPEC/Keck-II, when the comet was at 6.26 AU from the Sun and about 5.50 AU from Earth. With CRIRES, we detected five CO emission lines on several nights in each epoch, confirming the ubiquitous content and release of carbon monoxide from the nucleus. This is the first simultaneous detection of multiple lines from any (neutral) gaseous species in comet 29P at infrared wavelengths. It is also the first extraction of a rotational temperature based on the intensities of simultaneously measured spectral lines in 29P, and the retrieved rotational temperature is the lowest obtained in our infrared survey to date. We present the retrieved production rates (similar to 3 x 10(28) molecules s(-1)) and remarkably low (similar to 5 K) rotational temperatures for CO, and compare them with results from previous observations at radio wavelengths. Along with CO, we pursued detections of other volatiles, namely H2O, C2H6, C2H2, CH4, HCN, NH3, and CH3OH. Although they were not detected, we present sensitive upper limits. These results establish a new record for detections by infrared spectroscopy of parent volatiles in comets at large heliocentric distances. Until now considered to be a somewhat impossible task with IR ground-based facilities, these discoveries demonstrate new opportunities for targeting volatile species in distant comets.
C1 [Paganini, Lucas; Mumma, Michael J.; DiSanti, Michael A.; Villanueva, Geronimo L.; Bonev, Boncho P.] NASA GSFC, Goddard Ctr Astrobiol, Greenbelt, MD 20771 USA.
[Boehnhardt, Hermann; Lippi, Manuela] Max Planck Inst Sonnensyst Forsch, D-37191 Katlenburg Lindau, Germany.
[Villanueva, Geronimo L.; Bonev, Boncho P.] Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA.
[Kaeufl, Hans U.] ESO, D-85748 Garching, Germany.
[Blake, Geoffrey A.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA.
RP Paganini, L (reprint author), NASA GSFC, Goddard Ctr Astrobiol, MS 690, Greenbelt, MD 20771 USA.
EM lucas.paganini@nasa.gov
RI mumma, michael/I-2764-2013
FU NASA; NSF; Max-Planck-Gesellschaft; German-Israeli Foundation for
Scientific Research and Development
FX We thank the VLT science operations team of the European Southern
Observatory and the W.M. Keck Observatory for efficient operations of
the observatories. L.P. acknowledges Retha Pretorius, Jonathan Smoker
and Carla Aubel for their great assistance, and thanks Michael A'Hearn
and Martin Cordiner for helpful discussions. We are also grateful to
Zhong-Yi Lin and Josep Trigo-Rodriguez for providing magnitude
estimations, and to the anonymous referee for helpful comments. This
work was supported by NASA's Postdoctoral (L.P.), Planetary Astronomy
(PI:M.J.M. and PI:M.A.D.), and Astrobiology Programs (PI:M.J.M.), NSF
(PI:B.P.B.), the Max-Planck-Gesellschaft (H.B.), and the German-Israeli
Foundation for Scientific Research and Development (H.B. and M.L.).
NR 72
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PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD APR 1
PY 2013
VL 766
IS 2
AR 100
DI 10.1088/0004-637X/766/2/100
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 108UE
UT WOS:000316320900034
ER
PT J
AU Reynolds, MT
Loi, ST
Murphy, T
Miller, JM
Maitra, D
Gultekin, K
Gehrels, N
Kennea, JA
Siegel, MH
Gelbord, J
Kuin, P
Moss, V
Reeves, S
Robbins, WJ
Gaensler, BM
Reis, RC
Petre, R
AF Reynolds, Mark T.
Loi, Shyeh T.
Murphy, Tara
Miller, Jon M.
Maitra, Dipankar
Gueltekin, Kayhan
Gehrels, Neil
Kennea, Jamie A.
Siegel, Michael H.
Gelbord, Jonathan
Kuin, Paul
Moss, Vanessa
Reeves, Sarah
Robbins, William J.
Gaensler, B. M.
Reis, Rubens C.
Petre, Robert
TI G306.3-0.9: A NEWLY DISCOVERED YOUNG GALACTIC SUPERNOVA REMNANT
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE ISM: individual objects: (G306.3-0.9); ISM: supernova remnants
ID LARGE-MAGELLANIC-CLOUD; X-RAY SPECTROSCOPY; SOURCE CATALOG; EXPLOSION;
ABUNDANCES; EMISSION; PULSARS; MODELS; PLANE; N132D
AB We present X-ray and radio observations of the new Galactic supernova remnant (SNR) G306.3-0.9, recently discovered by Swift. Chandra imaging reveals a complex morphology, dominated by a bright shock. The X-ray spectrum is broadly consistent with a young SNR in the Sedov phase, implying an age of 2500 yr for a distance of 8 kpc, plausibly identifying this as one of the 20 youngest Galactic SNRs. Australia Telescope Compact Array imaging reveals a prominent ridge of radio emission that correlates with the X-ray emission. We find a flux density of similar to 160 mJy at 1 GHz, which is the lowest radio flux recorded for a Galactic SNR to date. The remnant is also detected at 24 mu m, indicating the presence of irradiated warm dust. The data reveal no compelling evidence for the presence of a compact stellar remnant.
C1 [Reynolds, Mark T.; Miller, Jon M.; Maitra, Dipankar; Gueltekin, Kayhan; Reis, Rubens C.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA.
[Loi, Shyeh T.; Murphy, Tara; Moss, Vanessa; Reeves, Sarah; Robbins, William J.; Gaensler, B. M.] Univ Sydney, Sch Phys, Sydney Inst Astron SIfA, Sydney, NSW 2006, Australia.
[Murphy, Tara] Univ Sydney, Sch Informat Technol, Sydney, NSW 2006, Australia.
[Gehrels, Neil; Petre, Robert] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Kennea, Jamie A.; Siegel, Michael H.; Gelbord, Jonathan] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA.
[Kuin, Paul] Univ Coll London, Mullard Space Sci Lab, Dorking RH5 6NT, Surrey, England.
RP Reynolds, MT (reprint author), Univ Michigan, Dept Astron, 500 Church St, Ann Arbor, MI 48109 USA.
EM markrey@umich.edu
RI Gaensler, Bryan/F-8655-2010;
OI Loi, Shyeh Tjing/0000-0002-6528-4548; Murphy, Tara/0000-0002-2686-438X;
Moss, Vanessa/0000-0002-3005-9738; reis, rubens/0000-0002-6618-2412;
Gaensler, Bryan/0000-0002-3382-9558; Gultekin,
Kayhan/0000-0002-1146-0198
FU Commonwealth of Australia; Chandra guest investigator program
FX We acknowledge the use of public data from the Swift data archive. We
thank CXC director Harvey Tananbaum for his allocation of Director's
time. The ATCA is part of the ATNF which is funded by the Commonwealth
of Australia for operation as a National Facility managed by CSIRO.
J.M.M. acknowledges support through the Chandra guest investigator
program.
NR 37
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PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD APR 1
PY 2013
VL 766
IS 2
AR 112
DI 10.1088/0004-637X/766/2/112
PG 6
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 108UE
UT WOS:000316320900046
ER
PT J
AU Setvak, M
Bedka, K
Lindsey, DT
Sokol, A
Charvat, Z
St'astka, J
Wang, PK
AF Setvak, Martin
Bedka, Kristopher
Lindsey, Daniel T.
Sokol, Alois
Charvat, Zdenek
St'astka, Jindrich
Wang, Pao K.
TI A-Train observations of deep convective storm tops
SO ATMOSPHERIC RESEARCH
LA English
DT Article
DE Convective storm; Storm-top; Overshooting top; Cold-ring shape; Cold-U
shape; Enhanced-V feature; Lower stratosphere; A-Train, CloudSat;
CALIPSO; MODIS
ID 3-DIMENSIONAL NUMERICAL-SIMULATION; OKLAHOMA TORNADIC STORMS;
UPPER-LEVEL STRUCTURE; SATELLITE-OBSERVATIONS; BRIGHTNESS TEMPERATURES;
WATER-VAPOR; THUNDERSTORM; CLOUDS; STRATOSPHERE; DYNAMICS
AB The paper highlights simultaneous observations of tops of deep convective clouds from several space-borne instruments including the Moderate Resolution Imaging Spectroradiometer (MODIS) of the Aqua satellite, Cloud Profiling Radar (CPR) of the CloudSat satellite, and Cloud-Aerosol Lidar with Orthogonal Polarization (CALIOP) flown on the CALIPSO satellite. These satellites share very close orbits, thus together with several other satellites they are referred to as the "A-Train" constellation. Though the primary responsibility of these satellites and their instrumentation is much broader than observations of fine-scale processes atop convective storms, in this study we document how data from the A-Train can contribute to a better understanding and interpretation of various storm-top features, such as overshooting tops, cold-U/V and cold ring features with their coupled embedded warm areas, above anvil ice plumes and jumping cirrus. The relationships between MODIS multi-spectral brightness temperature difference (BTD) fields and cloud top signatures observed by the CPR and CALIOP are also examined in detail to highlight the variability in BTD signals across convective storm events. (C) 2012 Elsevier B.V. All rights reserved.
C1 [Setvak, Martin; Charvat, Zdenek; St'astka, Jindrich] Czech Hydrometeorol Inst, Prague, Czech Republic.
[Bedka, Kristopher] NASA, Langley Res Ctr, Sci Syst & Applicat Inc, Hampton, VA 23665 USA.
[Lindsey, Daniel T.] NOAA, NESDIS, RAMMB, CIRA,CSU, Ft Collins, CO USA.
[Sokol, Alois] Comenius Univ, Fac Math Phys & Informat, Bratislava, Slovakia.
[St'astka, Jindrich] Charles Univ Prague, Fac Math & Phys, Prague, Czech Republic.
[Wang, Pao K.] Univ Wisconsin Madison, Madison, WI USA.
RP Setvak, M (reprint author), CHMI, Sabatce 17, CZ-14306 Prague 4, Czech Republic.
EM setvak@chmi.cz
RI Lindsey, Dan/F-5607-2010
OI Lindsey, Dan/0000-0002-0967-5683
FU Grant Agency of the Czech Republic [205/07/0905]; Faculty of Mathematics
and Physics of the Charles University, Prague, Czech Republic
[SW-2011-263308]; Grant C/SSAI/ASAP Program [2626-08-021 Task 1-020CY4];
[NSF ATM-0729898]
FX The authors wish to acknowledge Mike Fromm (Naval Research Laboratory,
Washington, D.C.) and Louie Grasso (Cooperative Institute for Research
in the Atmosphere, Ft. Collins, CO) for their valuable comments,
suggestions and/or long-term support of this study, as well as NASA,
NOAA and EUMETSAT for their data used in this study. Parts of this
research were carried out under support of the Grant Agency of the Czech
Republic, project 205/07/0905; Grant SW-2011-263308 of the Faculty of
Mathematics and Physics of the Charles University, Prague, Czech
Republic; Grant NSF ATM-0729898; and Grant C/SSAI/ASAP 2010 Program,
Contract # 2626-08-021 Task 1-020CY4.
NR 43
TC 17
Z9 17
U1 0
U2 23
PU ELSEVIER SCIENCE INC
PI NEW YORK
PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA
SN 0169-8095
J9 ATMOS RES
JI Atmos. Res.
PD APR 1
PY 2013
VL 123
SI SI
BP 229
EP 248
DI 10.1016/j.atmosres.2012.06.020
PG 20
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 112GL
UT WOS:000316580600019
ER
PT J
AU Bala, G
Krishna, S
Narayanappa, D
Cao, L
Caldeira, K
Nemani, R
AF Bala, G.
Krishna, Sujith
Narayanappa, Devaraju
Cao, Long
Caldeira, Ken
Nemani, Ramakrishna
TI An estimate of equilibrium sensitivity of global terrestrial carbon
cycle using NCAR CCSM4
SO CLIMATE DYNAMICS
LA English
DT Article
DE Climate change; Terrestrial carbon cycle; CO2-physiological effect;
CO2-fertilization; Carbon cycle feedback
ID FUTURE CLIMATE-CHANGE; COUPLED CLIMATE; ATMOSPHERIC CO2; VEGETATION
MODELS; SOIL RESPIRATION; DIOXIDE; FEEDBACKS; ECOSYSTEM; FERTILIZATION;
DYNAMICS
AB Increasing concentrations of atmospheric CO2 influence climate, terrestrial biosphere productivity and ecosystem carbon storage through its radiative, physiological and fertilization effects. In this paper, we quantify these effects for a doubling of CO2 using a low resolution configuration of the coupled model NCAR CCSM4. In contrast to previous coupled climate-carbon modeling studies, we focus on the near-equilibrium response of the terrestrial carbon cycle. For a doubling of CO2, the radiative effect on the physical climate system causes global mean surface air temperature to increase by 2.14 K, whereas the physiological and fertilization on the land biosphere effects cause a warming of 0.22 K, suggesting that these later effects increase global warming by about 10 % as found in many recent studies. The CO2-fertilization leads to total ecosystem carbon gain of 371 Gt-C (28 %) while the radiative effect causes a loss of 131 Gt-C (10 %) indicating that climate warming damps the fertilization-induced carbon uptake over land. Our model-based estimate for the maximum potential terrestrial carbon uptake resulting from a doubling of atmospheric CO2 concentration (285-570 ppm) is only 242 Gt-C. This highlights the limited storage capacity of the terrestrial carbon reservoir. We also find that the terrestrial carbon storage sensitivity to changes in CO2 and temperature have been estimated to be lower in previous transient simulations because of lags in the climate-carbon system. Our model simulations indicate that the time scale of terrestrial carbon cycle response is greater than 500 years for CO2-fertilization and about 200 years for temperature perturbations. We also find that dynamic changes in vegetation amplify the terrestrial carbon storage sensitivity relative to a static vegetation case: because of changes in tree cover, changes in total ecosystem carbon for CO2-direct and climate effects are amplified by 88 and 72 %, respectively, in simulations with dynamic vegetation when compared to static vegetation simulations.
C1 [Bala, G.; Krishna, Sujith; Narayanappa, Devaraju] Indian Inst Sci, Divecha Ctr Climate Change, Ctr Atmospher & Ocean Sci, Bangalore 560012, Karnataka, India.
[Cao, Long] Zhejiang Univ, Dept Earth Sci, Hangzhou 310027, Peoples R China.
[Caldeira, Ken] Carnegie Inst, Dept Global Ecol, Stanford, CA 94305 USA.
[Nemani, Ramakrishna] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
RP Bala, G (reprint author), Indian Inst Sci, Divecha Ctr Climate Change, Ctr Atmospher & Ocean Sci, Bangalore 560012, Karnataka, India.
EM bala.gov@gmail.com
RI Caldeira, Ken/E-7914-2011;
OI krishnakumar, sujith/0000-0001-7429-2809
FU Department of Science and Technology [DST 0948]; Divecha Center for
Climate Change
FX We thank Drs. Chris Jones and Sam Levis for their critical comments and
suggestions which helped us to improve the original manuscript
substantially. Financial support from Department of Science and
Technology under the grant DST 0948 is gratefully acknowledged. Dr.
Devaraju and Mr. Krishna are supported by the Divecha Center for Climate
Change.
NR 57
TC 6
Z9 6
U1 1
U2 29
PU SPRINGER
PI NEW YORK
PA 233 SPRING ST, NEW YORK, NY 10013 USA
SN 0930-7575
J9 CLIM DYNAM
JI Clim. Dyn.
PD APR
PY 2013
VL 40
IS 7-8
BP 1671
EP 1686
DI 10.1007/s00382-012-1495-9
PG 16
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 119CV
UT WOS:000317075700007
ER
PT J
AU Redfern, JV
Mckenna, MF
Moore, TJ
Calambokidis, J
Deangelis, ML
Becker, EA
Barlow, J
Forney, KA
Fiedler, PC
Chivers, SJ
AF Redfern, J. V.
Mckenna, M. F.
Moore, T. J.
Calambokidis, J.
Deangelis, M. L.
Becker, E. A.
Barlow, J.
Forney, K. A.
Fiedler, P. C.
Chivers, S. J.
TI Assessing the Risk of Ships Striking Large Whales in Marine Spatial
Planning
SO CONSERVATION BIOLOGY
LA English
DT Article
DE commercial shipping; generalized additive models; habitat modeling; risk
analysis
ID EASTERN NORTH PACIFIC; ATLANTIC RIGHT WHALES; CALIFORNIA CURRENT; BLUE;
ABUNDANCE; AUTOCORRELATION; HUMPBACK; ECOLOGY; HABITAT; MODEL
AB Marine spatial planning provides a comprehensive framework for managing multiple uses of the marine environment and has the potential to minimize environmental impacts and reduce conflicts among users. Spatially explicit assessments of the risks to key marine species from human activities are a requirement of marine spatial planning. We assessed the risk of ships striking humpback (Megaptera novaeangliae), blue (Balaenoptera musculus), and fin (Balaenoptera physalus) whales in alternative shipping routes derived from patterns of shipping traffic off Southern California (U.S.A.). Specifically, we developed whale-habitat models and assumed ship-strike risk for the alternative shipping routes was proportional to the number of whales predicted by the models to occur within each route. This definition of risk assumes all ships travel within a single route. We also calculated risk assuming ships travel via multiple routes. We estimated the potential for conflict between shipping and other uses (military training and fishing) due to overlap with the routes. We also estimated the overlap between shipping routes and protected areas. The route with the lowest risk for humpback whales had the highest risk for fin whales and vice versa. Risk to both species may be ameliorated by creating a new route south of the northern Channel Islands and spreading traffic between this new route and the existing route in the Santa Barbara Channel. Creating a longer route may reduce the overlap between shipping and other uses by concentrating shipping traffic. Blue whales are distributed more evenly across our study area than humpback and fin whales; thus, risk could not be ameliorated by concentrating shipping traffic in any of the routes we considered. Reducing ship-strike risk for blue whales may be necessary because our estimate of the potential number of strikes suggests that they are likely to exceed allowable levels of anthropogenic impacts established under U.S. laws.
C1 [Redfern, J. V.; Moore, T. J.; Barlow, J.; Fiedler, P. C.; Chivers, S. J.] Natl Ocean & Atmospher Adm, Protected Resources Div, SW Fisheries Sci Ctr, Natl Marine Fisheries Serv, La Jolla, CA 92037 USA.
[Mckenna, M. F.] Marine Mammal Commiss, Bethesda, MD 20814 USA.
[Calambokidis, J.] Cascadia Res, Olympia, WA 98501 USA.
[Deangelis, M. L.] Natl Ocean & Atmospher Adm, Protected Resources Div, Southwest Reg Off, Natl Marine Fisheries Serv, Long Beach, CA 90802 USA.
[Becker, E. A.; Forney, K. A.] Natl Ocean & Atmospher Adm, Protected Resources Div, SW Fisheries Sci Ctr, Natl Marine Fisheries Serv, Santa Cruz, CA 95060 USA.
RP Redfern, JV (reprint author), Natl Ocean & Atmospher Adm, Protected Resources Div, SW Fisheries Sci Ctr, Natl Marine Fisheries Serv, 8901 La Jolla Shores Dr, La Jolla, CA 92037 USA.
EM jessica.redfern@noaa.gov
OI Moore, Thomas/0000-0002-0243-6049
NR 33
TC 32
Z9 34
U1 2
U2 123
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 0888-8892
EI 1523-1739
J9 CONSERV BIOL
JI Conserv. Biol.
PD APR
PY 2013
VL 27
IS 2
BP 292
EP 302
DI 10.1111/cobi.12029
PG 11
WC Biodiversity Conservation; Ecology; Environmental Sciences
SC Biodiversity & Conservation; Environmental Sciences & Ecology
GA 113UN
UT WOS:000316694600008
PM 23521668
ER
PT J
AU Schimel, DS
Asner, GP
Moorcroft, P
AF Schimel, David S.
Asner, Gregory P.
Moorcroft, Paul
TI Observing changing ecological diversity in the Anthropocene
SO FRONTIERS IN ECOLOGY AND THE ENVIRONMENT
LA English
DT Review
ID REMOTE-SENSING DATA; CLIMATE-CHANGE; EVOLUTIONARY RESPONSES; NICHE;
FOREST; ECOSYSTEMS; BIOGEOCHEMISTRY; TEMPERATURE; SENSITIVITY;
TRANSITIONS
AB As the world enters the Anthropocene - a new geologic period, defined by humanity's massive impact on the planet - the Earth's rapidly changing environment is putting critical ecosystem services at risk. To understand and forecast how ecosystems will change over the coming decades, scientists will require an understanding of the sensitivity of species to environmental change. The current distribution of species and functional groups provides valuable information about the performance of various species in different environments. However, when the rate of environmental change is high, information inherent in the ranges of many species will disappear, since that information exists only under more or less steady-state conditions. The amount of information about species' relationships to climate declines as their distributions move farther from steady state. New remote-sensing technologies can map the chemical and structural traits of plant canopies and will allow for the inference of traits and, in many cases, species' ranges. Current satellite remote-sensing data can only produce relatively simple classifications, but new techniques will produce data with dramatically higher biological information content. Front Ecol Environ 2013;11(3):129-137, doi: 10.1890/120111 (published online 18 Jan 2013)
C1 [Schimel, David S.] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
[Asner, Gregory P.] Carnegie Inst Sci, Dept Global Ecol, Stanford, CA USA.
[Moorcroft, Paul] Harvard Univ, Dept Organism & Evolutionary Biol, Cambridge, MA 02138 USA.
RP Schimel, DS (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
EM david.schimel@jpl.nasa.gov
RI Asner, Gregory/G-9268-2013
OI Asner, Gregory/0000-0001-7893-6421
FU NASA; Gordon and Betty Moore Foundation; John D and Catherine T
MacArthur Foundation; WM Keck Foundation; Margaret A Cargill Foundation;
Grantham Foundation for the Protection of the Environment; Mary Anne
Nyburg Baker and G Leonard Baker Jr; William R Hearst III; NEON; NEON
airborne science team; NSF
FX This paper emerged from a workshop convened at the Carnegie Institution
for Science (Stanford, California) in 2010, and was supported by NASA.
The Carnegie Airborne Observatory is supported by the Gordon and Betty
Moore Foundation, the John D and Catherine T MacArthur Foundation, the
WM Keck Foundation, the Margaret A Cargill Foundation, the Grantham
Foundation for the Protection of the Environment, Mary Anne Nyburg Baker
and G Leonard Baker Jr, and William R Hearst III. DSS acknowledges
financial support from NEON and contributions from the NEON airborne
science team. NEON is sponsored by the NSF. Part of this work was
performed at the Jet Propulsion Laboratory, California Institute of
Technology, under a contract with NASA.
NR 54
TC 39
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U1 6
U2 134
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 1540-9295
EI 1540-9309
J9 FRONT ECOL ENVIRON
JI Front. Ecol. Environ.
PD APR
PY 2013
VL 11
IS 3
BP 129
EP 137
DI 10.1890/120111
PG 9
WC Ecology; Environmental Sciences
SC Environmental Sciences & Ecology
GA 117DL
UT WOS:000316932200015
ER
PT J
AU Holt, AL
Gagnon, Y
Vahidinia, S
Morse, DE
Sweeney, AM
AF Holt, A. L.
Gagnon, Y.
Vahidinia, S.
Morse, D. E.
Sweeney, A. M.
TI Photonic enhancement of symbiotic photosynthesis in giant clams
SO INTEGRATIVE AND COMPARATIVE BIOLOGY
LA English
DT Meeting Abstract
CT Annual Meeting of the Society-for-Integrative-and-Comparative-Biology
(SICB)
CY JAN 03-07, 2013
CL San Francisco, CA
SP Soc Integrat & Comparat Biol (SICB)
C1 Duke Univ, Durham, NC 27706 USA.
NASA Ames, Ames, IA USA.
Univ Penn, Philadelphia, PA 19104 USA.
EM holt@lifesci.ucsb.edu
RI Gagnon, Yakir/C-2665-2008
OI Gagnon, Yakir/0000-0003-2512-4520
NR 0
TC 0
Z9 0
U1 0
U2 7
PU OXFORD UNIV PRESS INC
PI CARY
PA JOURNALS DEPT, 2001 EVANS RD, CARY, NC 27513 USA
SN 1540-7063
J9 INTEGR COMP BIOL
JI Integr. Comp. Biol.
PD APR
PY 2013
VL 53
SU 1
BP E95
EP E95
PG 1
WC Zoology
SC Zoology
GA 117ZG
UT WOS:000316991400381
ER
PT J
AU Burow, LC
Woebken, D
Marshall, IPG
Lindquist, EA
Bebout, BM
Prufert-Bebout, L
Hoehler, TM
Tringe, SG
Pett-Ridge, J
Weber, PK
Spormann, AM
Singer, SW
AF Burow, Luke C.
Woebken, Dagmar
Marshall, Ian P. G.
Lindquist, Erika A.
Bebout, Brad M.
Prufert-Bebout, Leslie
Hoehler, Tori M.
Tringe, Susannah G.
Pett-Ridge, Jennifer
Weber, Peter K.
Spormann, Alfred M.
Singer, Steven W.
TI Anoxic carbon flux in photosynthetic microbial mats as revealed by
metatranscriptomics
SO ISME JOURNAL
LA English
DT Article
DE metatranscriptomics; NanoSIMS; anoxic carbon flux; fermentation;
glycogen
ID YELLOWSTONE-NATIONAL-PARK; COMMUNITY STRUCTURE; COASTAL
BACTERIOPLANKTON; CYANOBACTERIAL MATS; HYDROGEN-PRODUCTION;
BAJA-CALIFORNIA; GUERRERO NEGRO; BACTERIA; SEQUENCES; REMOVAL
AB Photosynthetic microbial mats possess extraordinary phylogenetic and functional diversity that makes linking specific pathways with individual microbial populations a daunting task. Close metabolic and spatial relationships between Cyanobacteria and Chloroflexi have previously been observed in diverse microbial mats. Here, we report that an expressed metabolic pathway for the anoxic catabolism of photosynthate involving Cyanobacteria and Chloroflexi in microbial mats can be reconstructed through metatranscriptomic sequencing of mats collected at Elkhorn Slough, Monterey Bay, CA, USA. In this reconstruction, Microcoleus spp., the most abundant cyanobacterial group in the mats, ferment photosynthate to organic acids, CO2 and H-2 through multiple pathways, and an uncultivated lineage of the Chloroflexi take up these organic acids to store carbon as polyhydroxyalkanoates. The metabolic reconstruction is consistent with metabolite measurements and single cell microbial imaging with fluorescence in situ hybridization and NanoSIMS. The ISME Journal (2013) 7, 817-829; doi:10.1038/ismej.2012.150; published online 29 November 2012
C1 [Burow, Luke C.; Woebken, Dagmar; Marshall, Ian P. G.; Spormann, Alfred M.] Stanford Univ, Dept Chem Engn, Stanford, CA 94305 USA.
[Burow, Luke C.; Woebken, Dagmar; Marshall, Ian P. G.; Spormann, Alfred M.] Stanford Univ, Dept Civil & Environm Engn, Stanford, CA 94305 USA.
[Burow, Luke C.; Woebken, Dagmar; Bebout, Brad M.; Prufert-Bebout, Leslie; Hoehler, Tori M.] NASA, Ames Res Ctr, Exobiol Branch, Moffett Field, CA 94035 USA.
[Lindquist, Erika A.; Tringe, Susannah G.] Joint Genome Inst, Walnut Creek, CA USA.
[Pett-Ridge, Jennifer; Weber, Peter K.] Lawrence Livermore Natl Lab, Phys & Life Sci Directorate, Livermore, CA USA.
[Singer, Steven W.] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Div Earth Sci, Berkeley, CA 94720 USA.
RP Singer, SW (reprint author), Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Div Earth Sci, 1 Cyclotron Rd,Mail Stop 74-316C, Berkeley, CA 94720 USA.
EM SWSinger@lbl.gov
RI Woebken, Dagmar/A-4447-2013;
OI Tringe, Susannah/0000-0001-6479-8427; Woebken,
Dagmar/0000-0002-1314-9926
FU US Department of Energy (DOE) Genomic Science Program [SCW1039]; US
Department of Energy at Lawrence Livermore National Laboratory
[DE-AC52-07NA27344]; US Department of Energy at Lawrence Berkeley
National Laboratory [DE-AC02-05CH11231]; Office of Science of the US
Department of Energy [DE-AC02-05CH11231]; German Research Foundation
(Deutsche Forschungsgemeinschaft)
FX Funding was provided by the US Department of Energy (DOE) Genomic
Science Program under contract SCW1039. Work at LLNL was performed under
the auspices of the US Department of Energy at Lawrence Livermore
National Laboratory under Contract DE-AC52-07NA27344. Work at LBNL was
performed under the auspices of the US Department of Energy at Lawrence
Berkeley National Laboratory under Contract DE-AC02-05CH11231. Pyrotag
and metatranscriptomic sequencing were conducted by the Joint Genome
Institute, which is supported by the Office of Science of the US
Department of Energy under Contract No. DE-AC02-05CH11231. DW was funded
by the German Research Foundation (Deutsche Forschungsgemeinschaft). We
thank Jeff Cann, Associate Wildlife Biologist, Central Region,
California Department of Fish and Game for coordinating our access to
the Moss Landing Wildlife Area.
NR 57
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Z9 17
U1 6
U2 57
PU NATURE PUBLISHING GROUP
PI LONDON
PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND
SN 1751-7362
J9 ISME J
JI ISME J.
PD APR
PY 2013
VL 7
IS 4
BP 817
EP 829
DI 10.1038/ismej.2012.150
PG 13
WC Ecology; Microbiology
SC Environmental Sciences & Ecology; Microbiology
GA 114FZ
UT WOS:000316727800012
PM 23190731
ER
PT J
AU Taylor, PC
Loeb, NG
AF Taylor, Patrick C.
Loeb, Norman G.
TI Impact of Sun-Synchronous Diurnal Sampling on Tropical TOA Flux
Interannual Variability and Trends
SO JOURNAL OF CLIMATE
LA English
DT Article
ID OUTGOING LONGWAVE RADIATION; HYDROLOGIC-CYCLE; CLOUD; BUDGET
AB Satellite observations of the earth's radiation budget (ERB) are a critical component of the climate observing system. Recent observations have been made from sun-synchronous orbits, which provide excellent spatial coverage with global measurements twice daily but do not resolve the full diurnal cycle. Previous investigations show that significant errors can occur in time-averaged energy budgets from sun-synchronous orbits if diurnal variations are ignored. However, the impact of incomplete diurnal sampling on top-of-atmosphere (TOA) flux variability and trends has received less attention. A total of 68 months of 3-hourly tropical outgoing longwave radiation (OLR) and reflected shortwave radiation (RSW) fluxes from the Clouds and the Earth's Radiant Energy System (CERES) synoptic (SYN) data product is used to examine the impact of incomplete diurnal sampling on TOA flux variability. Tropical OLR and RSW interannual variability and trends derived from sun-synchronous time sampling consistent with the Terra satellite from 2000 to 2005 show no statistically significant differences at the 95% confidence level with those obtained at 3-hourly time sampling at both 1 degrees x 1 degrees and 10 degrees x 10 degrees regional scales, as well as for tropical means. Monthly, 3-hourly OLR composite anomalies are decomposed into diurnally uniform and diurnal cycle shape change contributions to explain the impact of sampling on observed TOA flux variability. Diurnally uniform contributions to OLR variability account for more than 80% of interannual OLR variability at 1 degrees x 1 degrees spatial scales. Diurnal cycle shape variations are most important in equatorial land regions, contributing up to 50% to OLR variability over Africa. At spatial scales of 10 degrees x 10 degrees or larger, OLR variance contributions from diurnal cycle shape changes remain smaller than 20%.
C1 [Taylor, Patrick C.; Loeb, Norman G.] NASA, Climate Sci Branch, Langley Res Ctr, Hampton, VA 23681 USA.
RP Taylor, PC (reprint author), NASA, Langley Res Ctr, 21 Langley Blvd,Mail Stop 420, Hampton, VA 23681 USA.
EM patrick.c.taylor@nasa.gov
RI Taylor, Patrick/D-8696-2015
OI Taylor, Patrick/0000-0002-8098-8447
NR 27
TC 8
Z9 8
U1 0
U2 12
PU AMER METEOROLOGICAL SOC
PI BOSTON
PA 45 BEACON ST, BOSTON, MA 02108-3693 USA
SN 0894-8755
J9 J CLIMATE
JI J. Clim.
PD APR
PY 2013
VL 26
IS 7
BP 2184
EP 2191
DI 10.1175/JCLI-D-12-00416.1
PG 8
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 117GL
UT WOS:000316941400003
ER
PT J
AU Van Weverberg, K
Vogelmann, AM
Lin, W
Luke, EP
Cialella, A
Minnis, P
Khaiyer, M
Boer, ER
Jensen, MP
AF Van Weverberg, K.
Vogelmann, A. M.
Lin, W.
Luke, E. P.
Cialella, A.
Minnis, P.
Khaiyer, M.
Boer, E. R.
Jensen, M. P.
TI The Role of Cloud Microphysics Parameterization in the Simulation of
Mesoscale Convective System Clouds and Precipitation in the Tropical
Western Pacific
SO JOURNAL OF THE ATMOSPHERIC SCIENCES
LA English
DT Article
ID RESOLVING MODEL SIMULATIONS; CLIMATOLOGY PROJECT GPCP; MEASURING MISSION
TRMM; BULK ICE SCHEME; SATELLITE-OBSERVATIONS; OCEANIC CONVECTION; SIZE
DISTRIBUTIONS; PART II; EXPLICIT FORECASTS; RADIATIVE-TRANSFER
AB This paper presents a detailed analysis of convection-permitting cloud simulations, aimed at increasing the understanding of the role of parameterized cloud microphysics in the simulation of mesoscale convective systems (MCSs) in the tropical western Pacific (TWP). Simulations with three commonly used bulk microphysics parameterizations with varying complexity have been compared against satellite-retrieved cloud properties. An MCS identification and tracking algorithm was applied to the observations and the simulations to evaluate the number, spatial extent, and microphysical properties of individual cloud systems. Different from many previous studies, these individual cloud systems could be tracked over larger distances because of the large TWP domain studied.
The analysis demonstrates that the simulation of MCSs is very sensitive to the parameterization of microphysical processes. The most crucial element was found to be the fall velocity of frozen condensate. Differences in this fall velocity between the experiments were more related to differences in particle number concentrations than to fall speed parameterization. Microphysics schemes that exhibit slow sedimentation rates for ice aloft experience a larger buildup of condensate in the upper troposphere. This leads to more numerous and/or larger MCSs with larger anvils. Mean surface precipitation was found to be overestimated and insensitive to the microphysical schemes employed in this study. In terms of the investigated properties, the performances of complex two-moment schemes were not superior to the simpler one-moment schemes, since explicit prediction of number concentration does not necessarily improve processes such as ice nucleation, the aggregation of ice crystals into snowflakes, and their sedimentation characteristics.
C1 [Van Weverberg, K.; Vogelmann, A. M.; Lin, W.; Luke, E. P.; Cialella, A.; Jensen, M. P.] Brookhaven Natl Lab, Upton, NY 11973 USA.
[Van Weverberg, K.] Catholic Univ Louvain, Georges Lemaitre Ctr Earth & Climate Res TECLIM, BE-1348 Louvain, Belgium.
[Minnis, P.] NASA, Langley Res Ctr, Hampton, VA 23665 USA.
[Khaiyer, M.] Sci Syst & Applicat Inc, Hampton, VA USA.
[Boer, E. R.] Entropy Control Inc, La Jolla, CA USA.
RP Van Weverberg, K (reprint author), Catholic Univ Louvain, Georges Lemaitre Ctr Earth & Climate Res, Pl Louis Pasteur 3,SC10-L4-03-08, BE-1348 Louvain, Belgium.
EM kwinten.vanweverberg@uclouvain.be
RI Vogelmann, Andrew/M-8779-2014; Minnis, Patrick/G-1902-2010
OI Vogelmann, Andrew/0000-0003-1918-5423; Minnis,
Patrick/0000-0002-4733-6148
FU Laboratory Directed Research and Development Program at Brookhaven
National Laboratory; U.S. Department of Energy's Atmospheric Science
Program Atmospheric System Research (ASR); Office of Science Office of
Biological and Environmental Research program [DE-AC02-98CH10886]; Earth
System Modeling Program via the FASTER project; ASR [DE-SC0000991/003]
FX Research by Van Weverberg, Vogelmann, Lin, Luke, Cialella, and Jensen
was supported by the Laboratory Directed Research and Development
Program at Brookhaven National Laboratory, the U.S. Department of
Energy's Atmospheric Science Program Atmospheric System Research (ASR),
an Office of Science Office of Biological and Environmental Research
program, under Contract DE-AC02-98CH10886, and by the Earth System
Modeling Program via the FASTER project (www.bnl.gov/esm). M. Khaiyer
and P. Minnis were also supported by the ASR under Interagency Agreement
DE-SC0000991/003. We kindly acknowledge the use of the NY Blue: a Blue
Gene/L supercomputer that was used for the WRF simulations. We thank
three anonymous reviewers for their suggestions that led to major
improvements to the paper.
NR 82
TC 23
Z9 23
U1 2
U2 37
PU AMER METEOROLOGICAL SOC
PI BOSTON
PA 45 BEACON ST, BOSTON, MA 02108-3693 USA
SN 0022-4928
EI 1520-0469
J9 J ATMOS SCI
JI J. Atmos. Sci.
PD APR
PY 2013
VL 70
IS 4
BP 1104
EP 1128
DI 10.1175/JAS-D-12-0104.1
PG 25
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 118AC
UT WOS:000316993700008
ER
PT J
AU Odom, B
AF Odom, Brian
TI Great Lives from History: Scientists and Science
SO LIBRARY JOURNAL
LA English
DT Book Review
C1 [Odom, Brian] NASA, Marshall Space & Flight Ctr, Huntsville, AL 35811 USA.
RP Odom, B (reprint author), NASA, Marshall Space & Flight Ctr, Huntsville, AL 35811 USA.
NR 1
TC 0
Z9 0
U1 1
U2 1
PU REED BUSINESS INFORMATION
PI NEW YORK
PA 360 PARK AVENUE SOUTH, NEW YORK, NY 10010 USA
SN 0363-0277
J9 LIBR J
JI Libr. J.
PD APR 1
PY 2013
VL 138
IS 6
BP 102
EP 103
PG 2
WC Information Science & Library Science
SC Information Science & Library Science
GA 115XY
UT WOS:000316846400113
ER
PT J
AU Dobrokhodov, V
Xargay, E
Hovakimyan, N
Kaminer, I
Cao, CY
Gregory, IM
AF Dobrokhodov, Vladimir
Xargay, Enric
Hovakimyan, Naira
Kaminer, Isaac
Cao, Chengyu
Gregory, Irene M.
TI Multicriteria analysis of an L-1 adaptive flight control system
SO PROCEEDINGS OF THE INSTITUTION OF MECHANICAL ENGINEERS PART I-JOURNAL OF
SYSTEMS AND CONTROL ENGINEERING
LA English
DT Article
DE L-1 adaptive control; flying qualities; multicriteria optimization;
Pareto optimality; quasi-random sequences
AB This article presents an overview of the application of the Parameter Space Investigation method for the multicriteria design optimization of the L-1 adaptive flight control system implemented on the two turbine-powered dynamically-scaled generic transport model Airborne Subscale Transport Aircraft Research aircraft. In particular, this study addresses the improvement of a nominal prototype solution, obtained using basic design guidelines of L-1 adaptive control theory. The results validate the theoretical claims of L-1 adaptive control in terms of closed-loop performance and robustness and illustrate the systematic character of its design procedure. Furthermore, this article shows the suitability of the Parameter Space Investigation method for the multicriteria design optimization over a multidimensional design variable space of a flight control system subject to desired control specifications. The use of this particular method is of special interest, as it provides invaluable information about the behavior of the closed-loop system in an extended space of design parameters and performance criteria. The results and conclusions of this article have led to a deeper understanding of the characteristics of the closed-loop adaptive system and have contributed to the improvement of the flying qualities and the robustness margins of the adaptive L-1-augmented aircraft, which has been recently flight tested by National Aeronautics and Space Administration.
C1 [Dobrokhodov, Vladimir; Kaminer, Isaac] USN, Postgrad Sch, Dept Mech & Aerosp Engn, Monterey, CA 93943 USA.
[Xargay, Enric; Hovakimyan, Naira] Univ Illinois, Coordinated Sci Lab, Urbana, IL USA.
[Cao, Chengyu] Univ Connecticut, Dept Mech Engn, Storrs, CT USA.
[Gregory, Irene M.] NASA, Langley Res Ctr, Dynam Syst & Control Branch, Hampton, VA 23665 USA.
RP Dobrokhodov, V (reprint author), USN, Postgrad Sch, Dept Mech & Aerosp Engn, Monterey, CA 93943 USA.
EM vldobr@nps.edu
FU Air Force Office of Scientific Research; NASA
FX This study was supported by Air Force Office of Scientific Research and
NASA.
NR 22
TC 2
Z9 2
U1 0
U2 15
PU SAGE PUBLICATIONS LTD
PI LONDON
PA 1 OLIVERS YARD, 55 CITY ROAD, LONDON EC1Y 1SP, ENGLAND
SN 0959-6518
J9 P I MECH ENG I-J SYS
JI Proc. Inst. Mech. Eng. Part I-J Syst Control Eng.
PD APR
PY 2013
VL 227
IS I4
BP 413
EP 427
DI 10.1177/0959651812468545
PG 15
WC Automation & Control Systems
SC Automation & Control Systems
GA 121IC
UT WOS:000317235500004
ER
PT J
AU Liu, Y
Schuck, PW
AF Liu, Yang
Schuck, P. W.
TI A Note on Computation of Relative Magnetic-Helicity Flux Across the
Photosphere
SO SOLAR PHYSICS
LA English
DT Article
DE Solar magnetic field; Magnetic helicity; Helicity flux density
ID DYNAMICS-OBSERVATORY SDO; ACTIVE REGIONS; SOLAR CORONA; EVOLUTION;
ENERGY; INJECTION; IMAGER; TUBES; FIELD
AB A number of investigations of the rate of relative magnetic-helicity transport across the photosphere [] have reported differences in the estimates computed from two different formulations of the relative-helicity flux-density proxy G (A) and G (theta) . There have been suggestions that G (theta) is a more robust helicity-flux density proxy and that the differences in the estimates of are caused by biases in G (A), noise, and/or the boundary conditions. In this note, we prove that the differences are caused by the inconsistent choice of boundary conditions in the explicit or implicit Green's function [] used for computing G (A) and G (theta) when comparing the helicity-flux estimates based on G (A) and G (theta) . When the boundary conditions in are chosen consistently, the two helicity-flux density proxies, [G (A) and G (theta) ] produce essentially identical results for the rate of helicity transport across the photosphere. They also yield essentially identical results for the rate of helicity transport of the shearing and advection terms separately. Using MHD simulation, HMI observational data, and Monte Carlo simulations of noise we show that this result is robust. Neither the shape of the active region, nor the shape of the boundary, nor data noise causes any difference in the rate of helicity transport computed via G (A) and G (theta) .
C1 [Liu, Yang] Stanford Univ, WW Hansen Expt Phys Lab, Stanford, CA 94305 USA.
[Schuck, P. W.] NASA, Space Weather Lab, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Liu, Y (reprint author), Stanford Univ, WW Hansen Expt Phys Lab, Stanford, CA 94305 USA.
EM yliu@sun.stanford.edu; peter.schuck@nasa.gov
FU NASA [NAS5-02139 (HMI)]; NASA LWS grant; NASA HGI grant
FX We wish to thank P. Demoulin, E. Pariat, and K. Dalmasse for valuable
comments and suggestions. P. Demoulin suggested examining the size of
the padding area and the helicity density computed from the FFT. YL was
supported by NASA Contract NAS5-02139 (HMI) to Stanford University, and
PWS was supported by NASA LWS and HGI grants. The data have been used by
courtesy of NASA/SDO and the HMI science team.
NR 27
TC 4
Z9 4
U1 0
U2 5
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0038-0938
J9 SOL PHYS
JI Sol. Phys.
PD APR
PY 2013
VL 283
IS 2
BP 283
EP 294
DI 10.1007/s11207-012-0219-y
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 108BF
UT WOS:000316265100004
ER
PT J
AU Brown, ME
Hand, KP
AF Brown, M. E.
Hand, K. P.
TI SALTS AND RADIATION PRODUCTS ON THE SURFACE OF EUROPA
SO ASTRONOMICAL JOURNAL
LA English
DT Article
DE planets and satellites: composition; planets and satellites: individual
(Europa); planets and satellites: surfaces
ID INFRARED MAPPING SPECTROMETER; SULFURIC-ACID; WATER ICE; SUBSURFACE
OCEAN; GALILEO; SATELLITES; ATMOSPHERE; MINERALS; CHLORINE; IMPLANTATION
AB The surface of Europa could contain the compositional imprint of an underlying interior ocean, but competing hypotheses differ over whether spectral observations from the Galileo spacecraft show the signature of ocean evaporates or simply surface radiation products unrelated to the interior. Using adaptive optics at the W. M. Keck Observatory, we have obtained spatially resolved spectra of most of the disk of Europa at a spectral resolution similar to 40 times higher than seen by the Galileo spacecraft. These spectra show a previously undetected distinct signature of magnesium sulfate salts on Europa, but the magnesium sulfate is confined to the trailing hemisphere and spatially correlated with the presence of radiation products like sulfuric acid and SO2. On the leading, less irradiated, hemisphere, our observations rule out the presence of many of the proposed sulfate salts, but do show the presence of distorted water ice bands. Based on the association of the potential MgSO4 detection on the trailing side with other radiation products, we conclude that MgSO4 is also a radiation product, rather than a constituent of a Europa ocean brine. Based on ocean chemistry models, we hypothesize that, prior to irradiation, magnesium is primarily in the form of MgCl2, and we predict that NaCl and KCl are even more abundant, and, in fact, dominate the non-ice component of the leading hemisphere. We propose observational tests of this new hypothesis.
C1 [Brown, M. E.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA.
[Hand, K. P.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Brown, ME (reprint author), CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA.
EM mbrown@caltech.edu
FU Jet Propulsion Laboratory, California Institute of Technology under
National Aeronautics and Space Administration; internal Research and
Technology Development program; NASA Astrobiology Institute; Richard and
Barbara Rosenberg Professorship at the California Institute of
Technology
FX K.P.H. acknowledges support from the Jet Propulsion Laboratory,
California Institute of Technology, under a contract with the National
Aeronautics and Space Administration and funded in part through the
internal Research and Technology Development program. and from the NASA
Astrobiology Institute, through the "Astrobiology of Icy Worlds" node at
JPL. M. E. B. is supported by the Richard and Barbara Rosenberg
Professorship at the California Institute of Technology.
NR 47
TC 29
Z9 31
U1 5
U2 65
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-6256
J9 ASTRON J
JI Astron. J.
PD APR
PY 2013
VL 145
IS 4
AR 110
DI 10.1088/0004-6256/145/4/110
PG 7
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 107UW
UT WOS:000316247300024
ER
PT J
AU Grazier, KR
Newman, WI
Sharp, PW
AF Grazier, K. R.
Newman, W. I.
Sharp, P. W.
TI A MULTIRATE STORMER ALGORITHM FOR CLOSE ENCOUNTERS
SO ASTRONOMICAL JOURNAL
LA English
DT Article
DE celestial mechanics; methods: numerical; minor planets, asteroids:
general
ID N-BODY PROBLEM; SOLAR-SYSTEM; TIME-STEPS; INTEGRATIONS; EVOLUTION;
ORBITS
AB We present, analyze, and test a multirate Stormer-based algorithm for integrating close encounters when performing N-body simulations of the Sun, planets, and a large number of test particles. The algorithm is intended primarily for accurate simulations of the outer solar system. The algorithm uses stepsizes H and h(i), i = 1, ..., N-p, where h(i) << H and N-p is the number of planets. The stepsize H is used for the integration of the orbital motion of the Sun and planets at all times. H is also used as the stepsize for the integration of the orbital motion of test particles when they are not undergoing a close encounter. The stepsize h(i) is used to integrate the orbital motion of test particles during a close encounter with the ith planet. The position of the Sun and planets during a close encounter is calculated using Hermite interpolation. We tested the algorithm on two contrasting problems, and compared its performance with the existing method which uses the same stepsize for all bodies (this stepsize must be significantly smaller than H to ensure the close encounters are integrated accurately). Our tests show that the integration error for the new and existing methods are comparable when the stepsizes are chosen to minimize the error, and that for this choice of stepsizes the new method requires considerably less CPU time than the existing method.
C1 [Grazier, K. R.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Newman, W. I.] Univ Calif Los Angeles, Los Angeles, CA USA.
[Sharp, P. W.] Univ Auckland, Dept Math, Auckland, New Zealand.
RP Sharp, PW (reprint author), Univ Auckland, Dept Math, Private Bag 92019, Auckland, New Zealand.
EM kevin_grazier@yahoo.com; win@ucla.edu; sharp@math.auckland.ac.nz
OI Sharp, Philip/0000-0001-9550-0910
FU National Aeronautics and Space Administration; NeSI; Ministry of
Business, Innovation and Employment's Infrastructure programme
FX This work has been conducted in part at the Jet Propulsion Laboratory,
California Institute of Technology under a contract with the National
Aeronautics and Space Administration. Government sponsorship
acknowledged.; The authors thank the referee for the detailed report.
The referee's comments about the new method relative to the existing
method were especially invaluable. The authors wish to acknowledge the
contribution of the NeSI high-performance computing facilities and the
staff at the Centre for eResearch at the University of Auckland. New
Zealand's national facilities are provided by the New Zealand eScience
Infrastructure (NeSI) and funded jointly by NeSI's collaborator
institutions and through the Ministry of Business, Innovation and
Employment's Infrastructure programme (http://www.nesi.org.nz).
NR 18
TC 2
Z9 2
U1 1
U2 4
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-6256
J9 ASTRON J
JI Astron. J.
PD APR
PY 2013
VL 145
IS 4
AR 112
DI 10.1088/0004-6256/145/4/112
PG 8
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 107UW
UT WOS:000316247300026
ER
PT J
AU Howell, SB
Everett, ME
Seebode, SA
Szkody, P
Still, M
Wood, M
Ramsay, G
Cannizzo, J
Smale, A
AF Howell, Steve B.
Everett, Mark E.
Seebode, Sally A.
Szkody, Paula
Still, Martin
Wood, Matt
Ramsay, Gavin
Cannizzo, John
Smale, Alan
TI SPECTROSCOPY OF NEW AND POORLY KNOWN CATACLYSMIC VARIABLES IN THE KEPLER
FIELD
SO ASTRONOMICAL JOURNAL
LA English
DT Article
DE novae, cataclysmic variables
ID SU UMA-TYPE; V344 LYRAE; DWARF NOVAE; CATALOG; SUPERHUMPS; DISCOVERY;
ATLAS
AB The NASA Kepler mission has been in science operation since 2009 May and is providing high precision, high cadence light curves of over 150,000 targets. Prior to launch, nine cataclysmic variables were known to lie within Kepler's field of view. We present spectroscopy for seven systems, four of which were newly discovered since launch. All of the stars presented herein have been observed by, or are currently being observed by, the Kepler space telescope. Three historic systems and one new candidate could not be detected at their sky position and two candidates are called into question as to their true identity.
C1 [Howell, Steve B.; Still, Martin] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Everett, Mark E.] Natl Opt Astron Observ, Tucson, AZ 85719 USA.
[Seebode, Sally A.] San Mateo High Sch, San Mateo, CA 94401 USA.
[Szkody, Paula] Univ Washington, Dept Astron, Seattle, WA 98195 USA.
[Still, Martin] Bay Area Environm Res Inst Inc, West Sonoma, CA 95476 USA.
[Wood, Matt] Texas A&M Univ, Dept Phys & Astron, Commerce, TX 75429 USA.
[Ramsay, Gavin] Armagh Observ, Armagh BT61 9DG, North Ireland.
[Cannizzo, John] CRESST, Greenbelt, MD 20771 USA.
[Cannizzo, John] NASA GSFC, Astroparticle Phys Lab, Greenbelt, MD 20771 USA.
[Cannizzo, John] Univ Maryland, Dept Phys, Baltimore, MD 21250 USA.
[Smale, Alan] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Howell, SB (reprint author), NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
FU NSF [AST-1008734, AST-1109332]
FX We wish to thank the observatory staffs of Kitt Peak and Mount Palomar
for their help in carrying out the observations presented here. P. S.
acknowledges support from NSF grant AST-1008734. M. W. acknowledges
support from NSF grant AST-1109332. Kepler was competitively selected as
the 10th NASA Discovery mission.
NR 22
TC 12
Z9 12
U1 0
U2 3
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-6256
J9 ASTRON J
JI Astron. J.
PD APR
PY 2013
VL 145
IS 4
AR 109
DI 10.1088/0004-6256/145/4/109
PG 11
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 107UW
UT WOS:000316247300023
ER
PT J
AU Hand, KP
Brown, ME
AF Hand, K. P.
Brown, M. E.
TI KECK II OBSERVATIONS OF HEMISPHERICAL DIFFERENCES IN H2O2 ON EUROPA
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE astrochemistry; infrared: planetary systems; planets and satellites:
composition; planets and satellites: surfaces
ID ICY GALILEAN SATELLITES; HYDROGEN-PEROXIDE; WATER ICE; O-2; SURFACE;
ENERGY; LIFE; ION; TEMPERATURE; IRRADIATION
AB We present results from Keck II observations of Europa over four consecutive nights using the near-infrared spectrograph. Spectra were collected in the 3.14-4.0 mu m range, enabling detection and monitoring of the 3.5 mu m feature due to hydrogen peroxide. Galileo Near-Infrared Mapping Spectrometer results first revealed hydrogen peroxide on Europa in the anti-Jovian region of the leading hemisphere at a percent by number abundance of 0.13% +/- 0.07% relative to water. We find comparable results for the two nights over which we observed the leading hemisphere. Significantly, we observed a small amount of hydrogen peroxide (similar to 0.04%) during observations of Europa's anti-Jovian and sub-Jovian hemispheres. Almost no hydrogen peroxide was detected during observations of just the trailing hemisphere. We conclude that the Galileo observations likely represent the maximum hydrogen peroxide concentration, the exception potentially being the cold water ice regions of the poles, which are not readily observable from the ground. Our mapping of the peroxide abundance across Europa requires revisions to previous estimates for Europa's global surface abundance of oxidants and leads to a reduction in the total oxidant delivery expected for the subsurface ocean if an exchange of surface material with the ocean occurs.
C1 [Hand, K. P.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Brown, M. E.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91109 USA.
RP Hand, KP (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM khand@jpl.nasa.gov
FU NASA Planetary Astronomy program [NNX09AB49G]; NASA Astrobiology
Institute "Icy Worlds" node at JPL/Caltech
FX This research has been supported by grant NNX09AB49G from the NASA
Planetary Astronomy program and by the NASA Astrobiology Institute "Icy
Worlds" node at JPL/Caltech. The authors thank Robert W. Carlson for
helpful discussions.
NR 30
TC 9
Z9 9
U1 2
U2 30
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 2041-8205
J9 ASTROPHYS J LETT
JI Astrophys. J. Lett.
PD APR 1
PY 2013
VL 766
IS 2
AR L21
DI 10.1088/2041-8205/766/2/L21
PG 4
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 108UR
UT WOS:000316322200007
ER
PT J
AU Ryder, JW
Buxton, RE
Goetchius, E
Scott-Pandorf, M
Hackney, KJ
Fiedler, J
Ploutz-Snyder, RJ
Bloomberg, JJ
Ploutz-Snyder, LL
AF Ryder, Jeffrey W.
Buxton, Roxanne E.
Goetchius, Elizabeth
Scott-Pandorf, Melissa
Hackney, Kyle J.
Fiedler, James
Ploutz-Snyder, Robert J.
Bloomberg, Jacob J.
Ploutz-Snyder, Lori L.
TI Influence of muscle strength to weight ratio on functional task
performance
SO EUROPEAN JOURNAL OF APPLIED PHYSIOLOGY
LA English
DT Article
DE Muscle; Strength; Power; Work; Task performance
ID HUMAN SKELETAL-MUSCLE; PHYSICAL PERFORMANCE; SPACE; SPACEFLIGHT;
EXERCISE; MOBILITY; ADULTS; VOLUME; WOMEN; CHAIR
AB Existing models of muscle deconditioning such as bed rest are expensive and time-consuming. We propose a new model utilizing a weighted suit to manipulate muscle strength, power, or endurance relative to body weight. The aims of the study were to determine as to which muscle measures best predict functional task performance and to determine muscle performance thresholds below which task performance is impaired. Twenty subjects performed seven occupational astronaut tasks (supine and upright seat egress and walk, rise from fall, hatch opening, ladder climb, object carry, and construction board activity), while wearing a suit weighted with 0-120 % of body weight. Models of the relationship between muscle function/body weight and task completion time were developed using fractional polynomial regression and verified with pre- and post-flight astronaut performance data. Spline regression was used to identify muscle function thresholds for each task. Upright seat egress and walk was the most difficult task according to the spline regression analysis thresholds. Thresholds normalized to body weight were 17.8 N/kg for leg press isometric force, 17.6 W/kg for leg press power, 78.8 J/kg for leg press work, 5.9 N/kg isometric knee extension and 1.9 Nm/kg isokinetic knee extension torque. Leg press maximal isometric force/body weight was the most reliable measure for modeling performance of ambulatory tasks. Laboratory-based manipulation of relative strength has promise as an analog for spaceflight-induced loss of muscle function. Muscle performance values normalized to body weight can be used to predict occupational task performance and to establish relevant strength thresholds.
C1 [Ryder, Jeffrey W.; Fiedler, James; Ploutz-Snyder, Robert J.; Ploutz-Snyder, Lori L.] Univ Space Res Assoc, Houston, TX 77058 USA.
[Buxton, Roxanne E.; Goetchius, Elizabeth] Univ Houston, Houston, TX 77004 USA.
[Scott-Pandorf, Melissa; Hackney, Kyle J.] Wyle Integrated Sci & Engn, Houston, TX 77058 USA.
[Bloomberg, Jacob J.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA.
RP Ryder, JW (reprint author), Univ Space Res Assoc, Houston, TX 77058 USA.
EM jeffrey.ryder-1@nasa.gov
FU National Aeronautics and Space Administration Human Research Program
FX This work was supported by funding from the National Aeronautics and
Space Administration Human Research Program.
NR 21
TC 5
Z9 6
U1 2
U2 8
PU SPRINGER
PI NEW YORK
PA 233 SPRING ST, NEW YORK, NY 10013 USA
SN 1439-6319
J9 EUR J APPL PHYSIOL
JI Eur. J. Appl. Physiol.
PD APR
PY 2013
VL 113
IS 4
BP 911
EP 921
DI 10.1007/s00421-012-2500-z
PG 11
WC Physiology; Sport Sciences
SC Physiology; Sport Sciences
GA 106EI
UT WOS:000316124900012
PM 23011123
ER
PT J
AU Morrison, KD
Bristow, TF
Kennedy, MJ
AF Morrison, Keith D.
Bristow, Thomas F.
Kennedy, Martin J.
TI The reduction of structural iron in ferruginous smectite via the amino
acid cysteine: Implications for an electron shuttling compound
SO GEOCHIMICA ET COSMOCHIMICA ACTA
LA English
DT Article
ID COASTAL MARINE-SEDIMENTS; DIOCTAHEDRAL SMECTITES; CLAY-MINERALS;
QUANTITATIVE ASSAY; GEOBACTER-SULFURREDUCENS; FE(III) REDUCTION;
CRYSTAL-CHEMISTRY; HUMIC SUBSTANCES; METAL REDUCTION; OXIDATION
AB Microbes can reduce the structural iron (Fe(III)(str)) in clay minerals thus providing a potentially important terminal electron acceptor in the oxidation of organic matter. Many of these microorganisms participate in dissimilatory metal reduction with Fe(III) serving as the terminal electron acceptor either through direct contact with mineral surfaces or by way of electron shuttling compounds. Here we provide evidence for the electron shuttling capability of the amino acid cysteine with a ferruginous dioctahedral smectite (SWa-1) using infrared spectroscopy, X-ray diffraction and quantitative assay of ferric and ferrous iron. Reactions to determine the electron exchange between cysteine and SWa-1 were performed in pH 8 adjusted oxygen free solutions. Fourier transform infrared spectroscopy (FTIR) performed on self-supporting clay films reveals that cysteine has the ability to reduce Fe(III)(str), as shown by the decrease in the intensity of the AlFeOH and FeFeOH deformation and stretching bands resulting from decreased hydroxyl vibrations in the octahedral sheets. X-ray diffraction of the c-oriented SWa-1 reveals that cysteine intercalated into the d00l interlayer spaces. Quantitative iron assay indicates that the SWa-1 retains its structural iron upon reduction by cysteine and reoxidation. The increased interlayer spacing due to the intercalation of cysteine implies that this electron exchange is occurring from the basal surfaces of the smectite, as opposed to edge sites. When the SWa-1 was rinsed in dialysis tubing, the AlFeOH and FeFeOH vibrations reappear in FTIR spectra and the XRD patterns reveal that the cysteine no longer occupies interlayer sites. These results are consistent with partially reversible changes in clay mineral structure resulting from the reduction of Fe(III)(str). They support the hypothesis that cysteine could serve as an electron shuttling compound used by microorganisms to gain access to structural iron in clay minerals and extends the range of microbially mediated Fe redox reactions from iron oxides and oxyhydroxides to the largest pool of Fe in aquatic sediments, Fe-bearing clay minerals. (C) 2013 Published by Elsevier Ltd.
C1 [Morrison, Keith D.] Univ Calif Riverside, Dept Earth Sci, Riverside, CA 92521 USA.
[Bristow, Thomas F.] NASA, Exobiol Branch, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Kennedy, Martin J.] Univ Adelaide, Sch Earth & Environm Sci, Sprigg Geobiol Ctr, Adelaide, SA 5005, Australia.
RP Morrison, KD (reprint author), Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85287 USA.
EM keith.morrison@asu.edu
FU NSF Marine Sciences; ARC [DP110104367]
FX We would like to thank Eric Chronister and the University of California
Riverside, Department of Chemistry for help with the FTIR analysis and
interpretation. We thank Lynda Williams and Hilairy Hartnett for their
thorough evaluation of the manuscript and helpful discussions. This
research was supported by NSF Marine Sciences and ARC DP110104367.
NR 61
TC 5
Z9 5
U1 2
U2 58
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0016-7037
EI 1872-9533
J9 GEOCHIM COSMOCHIM AC
JI Geochim. Cosmochim. Acta
PD APR 1
PY 2013
VL 106
BP 152
EP 163
DI 10.1016/j.gca.2012.12.006
PG 12
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 100PP
UT WOS:000315713500010
ER
PT J
AU Benafan, O
Noebe, RD
Padula, SA
Gaydosh, DJ
Lerch, BA
Garg, A
Bigelow, GS
An, K
Vaidyanathan, R
AF Benafan, O.
Noebe, R. D.
Padula, S. A., II
Gaydosh, D. J.
Lerch, B. A.
Garg, A.
Bigelow, G. S.
An, K.
Vaidyanathan, R.
TI Temperature-dependent behavior of a polycrystalline NiTi shape memory
alloy around the transformation regime
SO SCRIPTA MATERIALIA
LA English
DT Article
DE Shape memory alloys; NiTi; Martensite reorientation; Dynamic modulus;
Neutron diffraction
ID MODULI
AB The mechanical and microstructural behavior of a polycrystalline Ni49.9Ti50.1 (at.%) shape memory alloy was investigated as a function of temperature around the transformation regime. The bulk macroscopic responses, measured using ex situ tensile deformation and impulse excitation tests, were compared to the microstructural evolution captured using in situ neutron diffraction. The onset stress for inelastic deformation and dynamic Young's modulus were found to decrease with temperature in the martensite regime followed by an increase starting near the austenite start temperature, attributed to the reverse transformation. Published by Elsevier Ltd. on behalf of Acta Materialia Inc.
C1 [Benafan, O.; Noebe, R. D.; Padula, S. A., II; Gaydosh, D. J.; Lerch, B. A.; Garg, A.; Bigelow, G. S.] NASA, Glenn Res Ctr, Struct & Mat Div, Cleveland, OH 44135 USA.
[Gaydosh, D. J.] Ohio Aerosp Inst, Cleveland, OH 44142 USA.
[Garg, A.] Univ Toledo, Toledo, OH 43606 USA.
[An, K.] Oak Ridge Natl Lab, Spallat Neutron Source, Oak Ridge, TN 37831 USA.
[Vaidyanathan, R.] Univ Cent Florida, Mat Sci & Engn Dept, Adv Mat Proc & Anal Ctr, Orlando, FL 32816 USA.
RP Benafan, O (reprint author), NASA, Glenn Res Ctr, Struct & Mat Div, Cleveland, OH 44135 USA.
EM othmane.benafan@nasa.gov
RI An, Ke/G-5226-2011
OI An, Ke/0000-0002-6093-429X
FU NASA Fundamental Aeronautics Program, Aeronautical Sciences and Fixed
Wing Projects; Division of Scientific User Facilities, Office of Basic
Energy Sciences, US Department of Energy [DE-AC05- 00OR22725]
FX Funding from the NASA Fundamental Aeronautics Program, Aeronautical
Sciences and Fixed Wing Projects is gratefully acknowledged. The authors
thank D.E. Nicholson and H.D. Skorpenske for technical support and
helpful discussions. This work has benefited from the use of the
Spallation Neutron Source at Oak Ridge National Laboratory, which is
funded by the Division of Scientific User Facilities, Office of Basic
Energy Sciences, US Department of Energy under Contract DE-AC05-
00OR22725 with UT-Battelle, LLC.
NR 11
TC 20
Z9 20
U1 2
U2 31
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 1359-6462
J9 SCRIPTA MATER
JI Scr. Mater.
PD APR
PY 2013
VL 68
IS 8
BP 571
EP 574
DI 10.1016/j.scriptamat.2012.11.042
PG 4
WC Nanoscience & Nanotechnology; Materials Science, Multidisciplinary;
Metallurgy & Metallurgical Engineering
SC Science & Technology - Other Topics; Materials Science; Metallurgy &
Metallurgical Engineering
GA 105CB
UT WOS:000316042100007
ER
PT J
AU Salim, WWAW
Zeitchek, MA
Hermann, AC
Ricco, AJ
Tan, M
Selch, F
Fleming, E
Bebout, BM
Bader, MM
ul Haque, A
Porterfield, DM
AF Salim, Wan W. Amani Wan
Zeitchek, Michael A.
Hermann, Andrew C.
Ricco, Antonio J.
Tan, Ming
Selch, Florian
Fleming, Erich
Bebout, Brad M.
Bader, Mamoun M.
ul Haque, Aeraj
Porterfield, D. Marshall
TI Multi-analyte Biochip (MAB) Based on All-solid-state Ion-selective
Electrodes (ASSISE) for Physiological Research
SO JOVE-JOURNAL OF VISUALIZED EXPERIMENTS
LA English
DT Article
DE Bioengineering; Issue 74; Medicine; Biomedical Engineering; Chemical
Engineering; Electrical Engineering; Mechanical Engineering; Chemistry;
Biochemistry; Anatomy; Physiology; Miniaturization; Microtechnology;
Electrochemical Techniques; electrochemical processes; astrobiology;
Analytical; Diagnostic and Therapeutic Techniques and Equipment;
Investigative Techniques; Technology; Industry; Agriculture;
electrochemical sensor; all-solid-state ion-selective electrode
(ASSISE); conductive polymer transducer;
poly(3,4-ethylenedioxythiophene) (PEDOT); lab-on-a-chip; Chlorella
vulgaris; photosynthesis; microfluidics
AB Lab-on-a-chip (LOC) applications in environmental, biomedical, agricultural, biological, and spaceflight research require an ion-selective electrode (ISE) that can withstand prolonged storage in complex biological media (1-4). An all-solid-state ion-selective-electrode (ASSISE) is especially attractive for the aforementioned applications. The electrode should have the following favorable characteristics: easy construction, low maintenance, and (potential for) miniaturization, allowing for batch processing. A microfabricated ASSISE intended for quantifying H+, Ca2+, and CO32- ions was constructed. It consists of a noble-metal electrode layer (i.e. Pt), a transduction layer, and an ion-selective membrane (ISM) layer. The transduction layer functions to transduce the concentration-dependent chemical potential of the ion-selective membrane into a measurable electrical signal.
The lifetime of an ASSISE is found to depend on maintaining the potential at the conductive layer/membrane interface 5-7. To extend the ASSISE working lifetime and thereby maintain stable potentials at the interfacial layers, we utilized the conductive polymer (CP) poly(3,4ethylenedioxythiophene) (PEDOT) 7-9 in place of silver/silver chloride (Ag/AgCl) as the transducer layer. We constructed the ASSISE in a lab-ona- chip format, which we called the multi-analyte biochip (MAB) (Figure 1).
Calibrations in test solutions demonstrated that the MAB can monitor pH (operational range pH 4-9), CO32-(measured range 0.01 mM (-1) mM), and Ca2+ (log-linear range 0.01 mM to 1 mM). The MAB for pH provides a near-Nernstian slope response after almost one month storage in algal medium. The carbonate biochips show a potentiometric profile similar to that of a conventional ion-selective electrode. Physiological measurements were employed to monitor biological activity of the model system, the microalga Chlorella vulgaris.
The MAB conveys an advantage in size, versatility, and multiplexed analyte sensing capability, making it applicable to many confined monitoring situations, on Earth or in space.
Biochip Design and Experimental Methods
The biochip is 10 x 11 mm in dimension and has 9 ASSISEs designated as working electrodes (WEs) and 5 Ag/AgCl reference electrodes (REs). Each working electrode (WE) is 240 mu m in diameter and is equally spaced at 1.4 mm from the REs, which are 480 mu m in diameter. These electrodes are connected to electrical contact pads with a dimension of 0.5 mm x 0.5 mm. The schematic is shown in Figure 2.
Cyclic voltammetry (CV) and galvanostatic deposition methods are used to electropolymerize the PEDOT films using a Bioanalytical Systems Inc. (BASI) C3 cell stand (Figure 3). The counter-ion for the PEDOT film is tailored to suit the analyte ion of interest. A PEDOT with poly(styrenesulfonate) counter ion (PEDOT/PSS) is utilized for H+ and CO32-, while one with sulphate (added to the solution as CaSO4) is utilized for Ca2+. The electrochemical properties of the PEDOT-coated WE is analyzed using CVs in redox-active solution (i.e. 2 mM potassium ferricyanide (K3Fe(CN)6)). Based on the CV profile, Randles-Sevcik analysis was used to determine the effective surface area (10). Spin-coating at 1,500 rpm is used to cast similar to 2 mu m thick ion-selective membranes (ISMs) on the MAB working electrodes (WEs).
The MAB is contained in a microfluidic flow-cell chamber filled with a 150 mu l volume of algal medium; the contact pads are electrically connected to the BASI system (Figure 4). The photosynthetic activity of Chlorella vulgaris is monitored in ambient light and dark conditions.
C1 [Salim, Wan W. Amani Wan; Zeitchek, Michael A.; Hermann, Andrew C.] Purdue Univ, Birck Bindley Physiol Sensing Facil, Dept Agr & Biol Engn, W Lafayette, IN 47907 USA.
[Ricco, Antonio J.; Tan, Ming; Selch, Florian; Fleming, Erich; Bebout, Brad M.] NASA Ames Res Ctr, Mountain View, CA USA.
[Bader, Mamoun M.] Penn State Univ Hazleton, Dept Chem, Hazleton, PA USA.
[ul Haque, Aeraj] Cooley LLP, Palo Alto, CA USA.
[Porterfield, D. Marshall] NASA Headquarters, NASA Life & Phys Sci, Human Explorat & Operat Miss Directorate, Washington, DC USA.
RP Salim, WWAW (reprint author), Purdue Univ, Birck Bindley Physiol Sensing Facil, Dept Agr & Biol Engn, W Lafayette, IN 47907 USA.
EM asalim@purdue.edu
FU NASA Astrobiology Science and Technology Instrument Development (ASTID)
[103498, 103692]; Birck Nantechnology Center at Purdue University for
wirebonding of the MAB devices; oon Hyeong Park for the CAD drawing of
the flow-cell chamber
FX We would like to thank NASA Astrobiology Science and Technology
Instrument Development (ASTID) Program for funding support (grant
numbers 103498 and 103692), Gale Lockwood of the Birck Nantechnology
Center at Purdue University for wirebonding of the MAB devices, and Joon
Hyeong Park for the CAD drawing of the flow-cell chamber.
NR 14
TC 0
Z9 0
U1 7
U2 26
PU JOURNAL OF VISUALIZED EXPERIMENTS
PI CAMBRIDGE
PA 1 ALEWIFE CENTER, STE 200, CAMBRIDGE, MA 02140 USA
SN 1940-087X
J9 JOVE-J VIS EXP
JI J. Vis. Exp.
PD APR
PY 2013
IS 74
AR UNSP e50020
DI 10.3791/50020
PG 10
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA V36QY
UT WOS:000209227100010
ER
PT J
AU Coggins, SB
Coops, NC
Hilker, T
Wulder, MA
AF Coggins, Sam B.
Coops, Nicholas C.
Hilker, Thomas
Wulder, Michael A.
TI Augmenting forest inventory attributes with geometric optical modelling
in support of regional susceptibility assessments to bark beetle
infestations
SO INTERNATIONAL JOURNAL OF APPLIED EARTH OBSERVATION AND GEOINFORMATION
LA English
DT Article
DE Landsat; Forest inventory; Mountain pine beetle; Susceptibility;
Geometric optical modelling; Western Canada; Lodgepole pine; Forest
health
ID MOUNTAIN PINE-BEETLE; RANGE EXPANSION; BOREAL FOREST; IMAGERY
AB Assessment of the susceptibility of forests to mountain pine beetle (Dendroctonus ponderosae Hopkins) infestation is based upon an understanding of the characteristics that predispose the stands to attack. These assessments are typically derived from conventional forest inventory data; however, this information often represents only managed forest areas. It does not cover areas such as forest parks or conservation regions and is often not regularly updated resulting in an inability to assess forest susceptibility. To address these shortcomings, we demonstrate how a geometric optical model (GOM) can be applied to Landsat-5 Thematic Mapper (TM) imagery (30 m spatial resolution) to estimate stand-level susceptibility to mountain pine beetle attack. Spectral mixture analysis was used to determine the proportion of sunlit canopy and background, and shadow of each Landsat pixel enabling per pixel estimates of attributes required for model inversion. Stand structural attributes were then derived from inversion of the geometric optical model and used as basis for susceptibility mapping. Mean stand density estimated by the geometric optical model was 2753 (standard deviation +/- 308) stems per hectare and mean horizontal crown radius was 2.09 (standard deviation +/- 0.11) metres. When compared to equivalent forest inventory attributes, model predictions of stems per hectare and crown radius were shown to be reasonably estimated using a Kruskal-Wallis ANOVA (p < 0.001). These predictions were then used to create a large area map that provided an assessment of the forest area susceptible to mountain pine beetle damage. (C) 2012 Elsevier B.V. All rights reserved.
C1 [Coggins, Sam B.; Coops, Nicholas C.] Univ British Columbia, Dept Forest Resources Management, Vancouver, BC V6T 1Z4, Canada.
[Hilker, Thomas] NASA, Goddard Space Flight Ctr, Biospher Sci Branch Code 618, Greenbelt, MD 20771 USA.
[Wulder, Michael A.] Nat Resources Canada, Canadian Forest Serv, Pacific Forestry Ctr, Victoria, BC, Canada.
RP Coops, NC (reprint author), Univ British Columbia, Dept Forest Resources Management, 2424 Main Mall, Vancouver, BC V6T 1Z4, Canada.
EM nicholas.coops@ubc.ca
RI Coops, Nicholas/J-1543-2012; Wulder, Michael/J-5597-2016
OI Coops, Nicholas/0000-0002-0151-9037; Wulder, Michael/0000-0002-6942-1896
FU Government of Canada; Pacific Forestry Centre; Natural Sciences and
Engineering Research Council (NSERC)
FX We acknowledge funding for this research from the following funding
agencies: (1) the Government of Canada, through the Mountain Pine Beetle
Program, a 6-year, $40 million program administered by Natural Resources
Canada - Canadian Forest Service; (2) the Pacific Forestry Centre
Graduate Student Award to Sam Coggins, administered by Natural Resources
Canada - Canadian Forest Service; and (3) a Natural Sciences and
Engineering Research Council (NSERC) grant to Nicholas Coops, supported
by the Government of Canada. Finally, we thank Peter Scarth for help at
the initial stages of the study in supplying code for the geometric
optical modelling.
NR 35
TC 3
Z9 3
U1 0
U2 32
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0303-2434
J9 INT J APPL EARTH OBS
JI Int. J. Appl. Earth Obs. Geoinf.
PD APR
PY 2013
VL 21
BP 444
EP 452
DI 10.1016/j.jag.2012.06.007
PG 9
WC Remote Sensing
SC Remote Sensing
GA 065IX
UT WOS:000313143100041
ER
PT J
AU Creamean, JM
Suski, KJ
Rosenfeld, D
Cazorla, A
DeMott, PJ
Sullivan, RC
White, AB
Ralph, FM
Minnis, P
Comstock, JM
Tomlinson, JM
Prather, KA
AF Creamean, Jessie M.
Suski, Kaitlyn J.
Rosenfeld, Daniel
Cazorla, Alberto
DeMott, Paul J.
Sullivan, Ryan C.
White, Allen B.
Ralph, F. Martin
Minnis, Patrick
Comstock, Jennifer M.
Tomlinson, Jason M.
Prather, Kimberly A.
TI Dust and Biological Aerosols from the Sahara and Asia Influence
Precipitation in the Western U.S.
SO SCIENCE
LA English
DT Article
ID ATMOSPHERIC ICE NUCLEI; OROGRAPHIC ENHANCEMENT; AIR-POLLUTION; LIQUID
WATER; MIXED-PHASE; CLOUD; PARTICLES; CLIMATE; SPECTROMETER; SUPPRESSION
AB Winter storms in California's Sierra Nevada increase seasonal snowpack and provide critical water resources and hydropower for the state. Thus, the mechanisms influencing precipitation in this region have been the subject of research for decades. Previous studies suggest Asian dust enhances cloud ice and precipitation, whereas few studies consider biological aerosols as an important global source of ice nuclei (IN). Here, we show that dust and biological aerosols transported from as far as the Sahara were present in glaciated high-altitude clouds coincident with elevated IN concentrations and ice-induced precipitation. This study presents the first direct cloud and precipitation measurements showing that Saharan and Asian dust and biological aerosols probably serve as IN and play an important role in orographic precipitation processes over the western United States.
C1 [Creamean, Jessie M.; Suski, Kaitlyn J.; Cazorla, Alberto; Prather, Kimberly A.] Univ Calif San Diego, Dept Chem & Biochem, La Jolla, CA 92093 USA.
[Rosenfeld, Daniel] Hebrew Univ Jerusalem, Inst Earth Sci, IL-91904 Jerusalem, Israel.
[DeMott, Paul J.] Colorado State Univ, Dept Atmospher Sci, Ft Collins, CO 80523 USA.
[Sullivan, Ryan C.] Carnegie Mellon Univ, Ctr Atmospher Particle Studies, Pittsburgh, PA 15213 USA.
[White, Allen B.; Ralph, F. Martin] NOAA, PSD, ESRL, Boulder, CO 80305 USA.
[Ralph, F. Martin; Prather, Kimberly A.] Univ Calif San Diego, SIO, La Jolla, CA 92093 USA.
[Minnis, Patrick] NASA, Langley Res Ctr, Hampton, VA 23681 USA.
[Comstock, Jennifer M.; Tomlinson, Jason M.] Pacific NW Natl Lab, Atmospher Sci & Global Change Div, Richland, WA 99352 USA.
RP Prather, KA (reprint author), Univ Calif San Diego, Dept Chem & Biochem, La Jolla, CA 92093 USA.
EM kprather@ucsd.edu
RI Sullivan, Ryan/B-4674-2008; DeMott, Paul/C-4389-2011; Tomlinson,
Jason/C-6566-2009; Rosenfeld, Daniel/F-6077-2016; Minnis,
Patrick/G-1902-2010;
OI Sullivan, Ryan/0000-0003-0701-7158; DeMott, Paul/0000-0002-3719-1889;
Rosenfeld, Daniel/0000-0002-0784-7656; Minnis,
Patrick/0000-0002-4733-6148; Creamean, Jessie/0000-0003-3819-5600
FU California Energy Commission [CEC 500-09-043]; Atmospheric System
Research (ASR)/U.S. Department of Energy (DOE) program; ASR/DOE program
[DE-SC0000991/003]; NASA MAPS Program
FX Funding was provided by the California Energy Commission under contract
CEC 500-09-043. D. R. was funded under the Atmospheric System Research
(ASR)/U.S. Department of Energy (DOE) program. P. M. was supported by
the ASR/DOE program under DE-SC0000991/003 and the NASA MAPS Program. J.
Mayer, E. Fitzgerald, D. Collins, and J. Cahill provided assistance with
UCSD/SIO equipment setup. The authors gratefully acknowledge the NOAA
Air Resources Laboratory (ARL) for the provision of the HYSPLIT
transport and dispersion model and READY website
(www.arl.noaa.gov/ready.php) used in this publication and the Office of
Naval Research for provision of NAAPS data. J. Ayers and R. Palikonda
(Science Systems and Applications) provided GOES-11 cloud top heights
used for HYSPLIT back trajectory analysis and %Ice in cloud. The
deployment of the NOAA and UCSD/SIO equipment at the Sugar Pine site
involved many field staff, particularly C. King (NOAA/ESRL/PSD). The
deployment of the DOE Gulfstream-1 involved many PNNL/Atmospheric
Radiation Measurement field staff, particularly E. Dukes, J. Hubbe, C.
Kluzek, H. Jonsson, M. Pekour, and B. Schmid. M. Hubbell and B. Svancara
flew the G-1 for the CalWater flight campaign. D. Collins and R.
Spackman provided insightful discussions during the editing stages of
this manuscript. T. Lersch of R. J. Lee provided TEM analyses of
collected IN. Data available in this paper are available in the
supplementary materials.
NR 44
TC 140
Z9 142
U1 15
U2 250
PU AMER ASSOC ADVANCEMENT SCIENCE
PI WASHINGTON
PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 USA
SN 0036-8075
J9 SCIENCE
JI Science
PD MAR 29
PY 2013
VL 339
IS 6127
BP 1572
EP 1578
DI 10.1126/science.1227279
PG 7
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 114HL
UT WOS:000316731600040
PM 23449996
ER
PT J
AU Pearse, J
Lundgren, P
AF Pearse, Jill
Lundgren, Paul
TI Source model of deformation at Lazufre volcanic center, central Andes,
constrained by InSAR time series
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
ID LONG VALLEY CALDERA; CAMPI-FLEGREI CALDERA; EASTERN CALIFORNIA; MAGMA
BODY; NEW-MEXICO; UPLIFT; INFLATION; SOCORRO; AREA
AB Recent interferometric synthetic aperture radar (InSAR) observations of the Lazufre region, central Andes, show large-scale uplift at a rate of about 3 cm/yr, beginning between 1998 and 2002. The initiation of this activity during the ERS satellite mission and its proximity to active volcanoes have made Lazufre the focus of several studies aimed at understanding its source geometry, its relation to nearby volcanoes, and whether or not the source area is expanding. There now exists a longer time series from multiple ERS/ENVISAT satellite tracks that allows a more comprehensive examination of the source geometry and its temporal and spatial variation, if any. We processed 15 years of InSAR data from three separate tracks; modeling the different look geometries provided greater resolution of source depth and geometry. We conclude that the source is a shallowly dipping sill at a depth of about 8 km, with no evidence of lateral expansion.
C1 [Pearse, Jill; Lundgren, Paul] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Pearse, Jill] Alberta Geol Survey, Edmonton, AB T6B 2X3, Canada.
RP Pearse, J (reprint author), Alberta Geol Survey, 4999 98 Ave NW, Edmonton, AB T6B 2X3, Canada.
EM jillpearse@gmail.com
FU National Aeronautics and Space Administration at the Jet Propulsion
Laboratory, California Institute of Technology
FX ERS and Envisat SAR data were provided courtesy of the European Space
Agency through M. Pritchard. The manuscript benefited from thoughtful
reviews by M. Shirzaei and M. Poland. The research described in this
paper was supported under contract with the National Aeronautics and
Space Administration at the Jet Propulsion Laboratory, California
Institute of Technology.
NR 25
TC 7
Z9 7
U1 1
U2 12
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0094-8276
J9 GEOPHYS RES LETT
JI Geophys. Res. Lett.
PD MAR 28
PY 2013
VL 40
IS 6
BP 1059
EP 1064
DI 10.1002/grl.50276
PG 6
WC Geosciences, Multidisciplinary
SC Geology
GA 148AY
UT WOS:000319215700007
ER
PT J
AU Zhang, CD
Gottschalck, J
Maloney, ED
Moncrieff, MW
Vitart, F
Waliser, DE
Wang, B
Wheeler, MC
AF Zhang, Chidong
Gottschalck, Jon
Maloney, Eric D.
Moncrieff, Mitchell W.
Vitart, Frederic
Waliser, Duane E.
Wang, Bin
Wheeler, Matthew C.
TI Cracking the MJO nut
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
ID MADDEN-JULIAN OSCILLATION; TROPICAL INTRASEASONAL OSCILLATION; ORGANIZED
CONVECTIVE SYSTEMS; GENERAL-CIRCULATION MODELS; CLOUD-RESOLVING MODEL;
SIMULATION DIAGNOSTICS; EQUATORIAL WAVES; WESTERN PACIFIC; FORECAST
SKILL; CLIMATE MODELS
AB The Madden-Julian oscillation poses great challenges to our understanding and prediction of tropical convection and the large-scale circulation. Several internationally coordinated activities were recently formed to meet the challenges from the perspectives of numerical simulations, prediction, diagnostics, and virtual and actual field campaigns. This article provides a brief description of these activities and their connections, with the motivation in part to encourage the next generation of physical scientists to help solve the grand challenging problem of the Madden-Julian oscillation.
C1 [Zhang, Chidong] Univ Miami, Miami, FL USA.
[Gottschalck, Jon] NOAA NCEP CPC, College Pk, MD USA.
[Maloney, Eric D.] Colorado State Univ, Ft Collins, CO 80523 USA.
[Moncrieff, Mitchell W.] NCAR, Boulder, CO USA.
[Vitart, Frederic] ECMWF, Reading, Berks, England.
[Waliser, Duane E.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Wang, Bin] Univ Hawaii, Honolulu, HI 96822 USA.
[Wheeler, Matthew C.] CAWCR, Melbourne, Vic, Australia.
RP Zhang, CD (reprint author), 4600 Rickenbacker Causeway, Miami, FL 33149 USA.
EM czhang@rsmas.miami.edu
RI Wheeler, Matthew/C-9038-2011; Maloney, Eric/A-9327-2008
OI Wheeler, Matthew/0000-0002-9769-1973; Maloney, Eric/0000-0002-2660-2611
FU NSF; NOAA; DOE; ONR; NASA; Bureau of Meteorology; CSIRO; National
Science Foundation
FX The authors thank George Kiladis for his constructive comments on an
earlier version of the manuscript. The writing of this article was
supported by grants and contracts from NSF, NOAA, DOE, ONR, and NASA.
DW's contribution was carried out on behalf of the Jet Propulsion
Laboratory, California Institute of Technology, under a contract with
NASA. The Centre for Australian Weather and Climate Research is a
partnership between the Bureau of Meteorology and CSIRO. The National
Center for Atmospheric Research is sponsored by the National Science
Foundation.
NR 75
TC 63
Z9 64
U1 2
U2 30
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0094-8276
J9 GEOPHYS RES LETT
JI Geophys. Res. Lett.
PD MAR 28
PY 2013
VL 40
IS 6
BP 1223
EP 1230
DI 10.1002/grl.50244
PG 8
WC Geosciences, Multidisciplinary
SC Geology
GA 148AY
UT WOS:000319215700037
ER
PT J
AU Baasandorj, M
Fleming, EL
Jackman, CH
Burkholder, JB
AF Baasandorj, Munkhbayar
Fleming, Eric L.
Jackman, Charles H.
Burkholder, James B.
TI O(D-1) Kinetic Study of Key Ozone Depleting Substances and Greenhouse
Gases
SO JOURNAL OF PHYSICAL CHEMISTRY A
LA English
DT Article
ID RATE COEFFICIENTS; ATMOSPHERIC CHEMISTRY; OH; HALOCARBONS; LIFETIMES
AB A key stratospheric loss process for ozone depleting substances (ODSs) and greenhouse gases (GHGs) is reaction with the O(D-1) atom. In this study, rate coefficients, k, for the O(D-1) atom reaction were measured for the following key halocarbons: chlorofluorocarbons (CFCs) CFCl3 (CFC-11), CF2Cl2 (CFC-12), CFCl2 center dot CF2Cl (CFC-113), CF2ClCF2Cl (CFC-114), CF3CF2Cl (CFC-115); hydrochlorofluorocarbons (HCFCs) CHF2Cl (HCFC-22), CH3CClF2 (HCFC-142b); and hydrofluorocarbons (HFCs) CHF3 (HFC-23), CHF2CF3 (HFC-125), CH3CF3 (HFC-143a), and CF3CHFCF3 (HFC-227ea). Total rate coefficients, k(T), corresponding to the loss of the O(D-1) atom, were measured over the temperature range 217-373 K using a competitive reactive technique. k(T) values for the CFC and HCFC reactions were >1 x 10(-10) cm(3) molecule(-1) s(-1), except for CFC-115, and the rate coefficients for the HFCs were in the range (0.095-0.72) x 10(-10) cm(3) molecule(-1) s(-1). Rate coefficients for the CFC-12, CFC-114, CFC-115, HFC-23, HFC-125, HFC-143a, and HFC-227ea reactions were observed to have a weak negative temperature dependence, E/R approximate to -25 K. Reactive rate coefficients, k(R), corresponding to the loss of the halocarbon, were measured for CFC-11, CFC-115, HCFC-22, HCFC-142b, HFC-23, HFC-125, HFC-143a, and HFC-227ea using a relative rate technique. The reactive branching ratio obtained was dependent on the composition of the halocarbon and the trend in O(D-1) reactivity with the extent of hydrogen and chlorine substitution is discussed. The present results are critically compared with previously reported kinetic data and the discrepancies are discussed. 2D atmospheric model calculations were used to evaluate the local and global annually averaged atmospheric lifetimes of the halocarbons and the contribution of O(D-1) chemistry to their atmospheric loss. The O(D-1) reaction was found to be a major global loss process for CFC-114 and CFC-115 and a secondary global loss process for the other molecules included in this study.
C1 [Baasandorj, Munkhbayar; Burkholder, James B.] NOAA, Earth Syst Res Lab, Div Chem Sci, Boulder, CO 80305 USA.
[Baasandorj, Munkhbayar] Univ Colorado, Cooperat Inst Res Environm Sci, Boulder, CO 80309 USA.
[Fleming, Eric L.; Jackman, Charles H.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Fleming, Eric L.] Sci Syst & Applicat Inc, Lanham, MD 20706 USA.
RP Burkholder, JB (reprint author), NOAA, Earth Syst Res Lab, Div Chem Sci, Boulder, CO 80305 USA.
EM James.B.Burkholder@noaa.gov
RI Burkholder, James/H-4914-2013; Jackman, Charles/D-4699-2012; Manager,
CSD Publications/B-2789-2015
FU NOAA's Climate Goal Program; NASA's Atmospheric Composition: Laboratory
Studies and Modeling and Analysis Program
FX This work was supported in part by NOAA's Climate Goal and NASA's
Atmospheric Composition: Laboratory Studies and Modeling and Analysis
Programs.
NR 20
TC 4
Z9 4
U1 3
U2 26
PU AMER CHEMICAL SOC
PI WASHINGTON
PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA
SN 1089-5639
J9 J PHYS CHEM A
JI J. Phys. Chem. A
PD MAR 28
PY 2013
VL 117
IS 12
BP 2434
EP 2445
DI 10.1021/jp312781c
PG 12
WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical
SC Chemistry; Physics
GA 118NO
UT WOS:000317032400004
PM 23441917
ER
PT J
AU Norris, RP
Afonso, J
Bacon, D
Beck, R
Bell, M
Beswick, RJ
Best, P
Bhatnagar, S
Bonafede, A
Brunetti, G
Budavari, T
Cassano, R
Condon, JJ
Cress, C
Dabbech, A
Feain, I
Fender, R
Ferrari, C
Gaensler, BM
Giovannini, G
Haverkorn, M
Heald, G
Van der Heyden, K
Hopkins, AM
Jarvis, M
Johnston-Hollitt, M
Kothes, R
Van Langevelde, H
Lazio, J
Mao, MY
Martinez-Sansigre, A
Mary, D
Mcalpine, K
Middelberg, E
Murphy, E
Padovani, P
Paragi, Z
Prandoni, I
Raccanelli, A
Rigby, E
Roseboom, IG
Rottgering, H
Sabater, J
Salvato, M
Scaife, AMM
Schilizzi, R
Seymour, N
Smith, DJB
Umana, G
Zhao, GB
Zinn, PC
AF Norris, Ray P.
Afonso, J.
Bacon, D.
Beck, Rainer
Bell, Martin
Beswick, R. J.
Best, Philip
Bhatnagar, Sanjay
Bonafede, Annalisa
Brunetti, Gianfranco
Budavari, Tamas
Cassano, Rossella
Condon, J. J.
Cress, Catherine
Dabbech, Arwa
Feain, I.
Fender, Rob
Ferrari, Chiara
Gaensler, B. M.
Giovannini, G.
Haverkorn, Marijke
Heald, George
Van der Heyden, Kurt
Hopkins, A. M.
Jarvis, M.
Johnston-Hollitt, Melanie
Kothes, Roland
Van Langevelde, Huib
Lazio, Joseph
Mao, Minnie Y.
Martinez-Sansigre, Alejo
Mary, David
Mcalpine, Kim
Middelberg, E.
Murphy, Eric
Padovani, P.
Paragi, Zsolt
Prandoni, I.
Raccanelli, A.
Rigby, Emma
Roseboom, I. G.
Rottgering, H.
Sabater, Jose
Salvato, Mara
Scaife, Anna M. M.
Schilizzi, Richard
Seymour, N.
Smith, Dan J. B.
Umana, Grazia
Zhao, G. -B.
Zinn, Peter-Christian
TI Radio Continuum Surveys with Square Kilometre Array Pathfinders
SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF AUSTRALIA
LA English
DT Article
DE radiotelescopes; surveys; galaxy evolution; cosmology
ID ACTIVE GALACTIC NUCLEI; DIGITAL-SKY-SURVEY; DEEP-FIELD-SOUTH;
STAR-FORMATION HISTORY; K-Z RELATION; PROBABILISTIC
CROSS-IDENTIFICATION; SPECTRAL ENERGY-DISTRIBUTIONS; INFRARED
EXTRAGALACTIC FIELD; BASE-LINE INTERFEROMETRY; SPITZER-SPACE-TELESCOPE
AB In the lead-up to the Square Kilometre Array (SKA) project, several next-generation radio telescopes and upgrades are already being built around the world. These include APERTIF (The Netherlands), ASKAP (Australia), e-MERLIN (UK), VLA (USA), e-EVN (based in Europe), LOFAR (The Netherlands), MeerKAT (South Africa), and the Murchison Widefield Array. Each of these new instruments has different strengths, and coordination of surveys between them can help maximise the science from each of them. A radio continuum survey is being planned on each of them with the primary science objective of understanding the formation and evolution of galaxies over cosmic time, and the cosmological parameters and large-scale structures which drive it. In pursuit of this objective, the different teams are developing a variety of new techniques, and refining existing ones. To achieve these exciting scientific goals, many technical challenges must be addressed by the survey instruments. Given the limited resources of the global radio-astronomical community, it is essential that we pool our skills and knowledge. We do not have sufficient resources to enjoy the luxury of re-inventing wheels. We face significant challenges in calibration, imaging, source extraction and measurement, classification and cross-identification, redshift determination, stacking, and data-intensive research. As these instruments extend the observational parameters, we will face further unexpected challenges in calibration, imaging, and interpretation. If we are to realise the full scientific potential of these expensive instruments, it is essential that we devote enough resources and careful study to understanding the instrumental effects and how they will affect the data. We have established an SKA Radio Continuum Survey working group, whose prime role is to maximise science from these instruments by ensuring we share resources and expertise across the projects. Here we describe these projects, their science goals, and the technical challenges which are being addressed to maximise the science return.
C1 [Norris, Ray P.; Feain, I.; Mao, Minnie Y.; Seymour, N.] CSIRO Astron & Space Sci, Epping, NSW 1710, Australia.
[Afonso, J.; Bell, Martin; Gaensler, B. M.] ARC Ctr Excellence All Sky Astrophys CAASTRO, Redfern, NSW 2016, Australia.
[Afonso, J.] Univ Lisbon, Observ Astron Lisboa, Ctr Astron & Astrofis, P-1349018 Lisbon, Portugal.
[Bacon, D.; Martinez-Sansigre, Alejo; Raccanelli, A.; Zhao, G. -B.] Univ Portsmouth, Inst Cosmol & Gravitat, Portsmouth PO1 3FX, Hants, England.
[Beck, Rainer] Max Planck Inst Radioastron, D-53121 Bonn, Germany.
[Bell, Martin; Fender, Rob; Scaife, Anna M. M.] Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England.
[Bell, Martin; Feain, I.; Gaensler, B. M.] Univ Sydney, Sch Phys, Sydney Inst Astron, Sydney, NSW 2006, Australia.
[Beswick, R. J.; Schilizzi, Richard] Univ Manchester, Jodrell Bank Ctr Astrophys, Sch Phys & Astron, Manchester M13 9PL, Lancs, England.
[Best, Philip; Sabater, Jose] Univ Edinburgh, Royal Observ, Inst Astron, Edinburgh EH9 3HJ, Midlothian, Scotland.
[Bhatnagar, Sanjay; Condon, J. J.] Natl Radio Astron Observ, Charlottesville, VA 22903 USA.
[Bonafede, Annalisa; Salvato, Mara] Max Planck Inst Plasma Phys, D-85748 Garching, Germany.
[Brunetti, Gianfranco; Cassano, Rossella; Giovannini, G.; Prandoni, I.] INAF IRA, I-40129 Bologna, Italy.
[Budavari, Tamas] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA.
[Cress, Catherine; Jarvis, M.] Univ Western Cape, Dept Phys, ZA-7535 Cape Town, South Africa.
[Dabbech, Arwa; Ferrari, Chiara; Mary, David] Univ Nice Sophia Antipolis, CNRS, Observ Cote Azur, Lab Lagrange,UMR 7293, F-06300 Nice, France.
[Haverkorn, Marijke; Van Langevelde, Huib; Rottgering, H.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands.
[Haverkorn, Marijke] Radboud Univ Nijmegen, Dept Astrophys IMAPP, NL-6500 GL Nijmegen, Netherlands.
[Heald, George] ASTRON, NL-7990 AA Dwingeloo, Netherlands.
[Van der Heyden, Kurt] Univ Cape Town, Dept Astron, Astrophys Cosmol & Grav Ctr, ZA-7701 Rondebosch, South Africa.
[Hopkins, A. M.; Mao, Minnie Y.] Australian Astron Observ, Epping, NSW 1710, Australia.
[Jarvis, M.; Mcalpine, Kim; Smith, Dan J. B.] Univ Hertfordshire, Sci & Technol Res Inst, Ctr Astrophys Res, Hatfield AL10 9AB, Herts, England.
[Jarvis, M.] Univ Oxford, Oxford OX1 3RH, England.
[Johnston-Hollitt, Melanie] Victoria Univ Wellington, Sch Chem & Phys Sci, Wellington 6140, New Zealand.
[Kothes, Roland] Natl Res Council Canada, Natl Sci Infrastruct, Domin Radio Astrophys Observ, Penticton, BC V2A 6J9, Canada.
[Van Langevelde, Huib] Joint Inst VLBI Europe, NL-7990 AA Dwingeloo, Netherlands.
[Lazio, Joseph; Raccanelli, A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Mao, Minnie Y.] Natl Radio Astron Observ, Socorro, NM 87801 USA.
[Mao, Minnie Y.] Univ Tasmania, Sch Math & Phys, Hobart, Tas 7001, Australia.
[Mcalpine, Kim] Rhodes Univ, Dept Phys & Elect, ZA-6140 Grahamstown, South Africa.
[Middelberg, E.; Zinn, Peter-Christian] Ruhr Univ Bochum, Astron Inst, D-44801 Bochum, Germany.
[Murphy, Eric] Carnegie Observ, Pasadena, CA 91101 USA.
[Padovani, P.] European So Observ, D-85748 Garching, Germany.
[Raccanelli, A.] CALTECH, Pasadena, CA 91125 USA.
[Rigby, Emma] Univ Nottingham, Sch Phys & Astron, Nottingham NG7 2RD, England.
[Umana, Grazia] INAF Catania Astrophys Observ, I-95123 Catania, Italy.
RP Norris, RP (reprint author), CSIRO Astron & Space Sci, POB 76, Epping, NSW 1710, Australia.
EM Ray.Norris@csiro.au
RI Norris, Ray/A-1316-2008; Afonso, Jose/B-5185-2013;
OI Norris, Ray/0000-0002-4597-1906; Afonso, Jose/0000-0002-9149-2973;
Raccanelli, Alvise/0000-0001-6726-0438; Prandoni,
Isabella/0000-0001-9680-7092; Umana, Grazia/0000-0002-6972-8388;
Cassano, Rossella/0000-0003-4046-0637; Brunetti,
Gianfranco/0000-0003-4195-8613; Giovannini,
Gabriele/0000-0003-4916-6362; Seymour, Nicholas/0000-0003-3506-5536; van
Langevelde, Huib Jan/0000-0002-0230-5946; Padovani,
Paolo/0000-0002-4707-6841; Paragi, Zsolt/0000-0002-5195-335X; Gaensler,
Bryan/0000-0002-3382-9558; Sabater, Jose/0000-0003-1149-6294
FU Australian Research Council Centre of Excellence for All-sky
Astrophysics (CAASTRO) [CE110001020]; Science and Technology Foundation
(FCT, Portugal) [PTDC/FIS/100170/2008, PTDC/CTE-AST/105287/2008,
PEst-OE/FIS/UI2751/2011]; Agence Nationale de la Recherche
[ANR-09-JCJC-0001-01]; Observatoire de la Cote d'Azur; Conseil regional
Provence-Alpes-Cote d'Azur
FX We are indebted to the Lorentz Center in Leiden for hosting and funding
the workshop in 2011 February, which gave rise to this paper. Parts of
this research were supported by the Australian Research Council Centre
of Excellence for All-sky Astrophysics (CAASTRO), through project number
CE110001020. Part of the research described in this paper was carried
out at the Jet Propulsion Laboratory, California Institute of
Technology, under contract with the National Aeronautics and Space
Administration. JA gratefully acknowledges support from the Science and
Technology Foundation (FCT, Portugal) through the research grants
PTDC/FIS/100170/2008, PTDC/CTE-AST/105287/2008, and
PEst-OE/FIS/UI2751/2011. CF and AD acknowledge financial support by the
Agence Nationale de la Recherche through grant ANR-09-JCJC-0001-01. AD
acknowledges financial support from the joint PhD program of
Observatoire de la Cote d'Azur and Conseil regional Provence-Alpes-Cote
d'Azur.
NR 465
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PI NEW YORK
PA 32 AVENUE OF THE AMERICAS, NEW YORK, NY 10013-2473 USA
SN 1323-3580
EI 1448-6083
J9 PUBL ASTRON SOC AUST
JI Publ. Astron. Soc. Aust.
PD MAR 27
PY 2013
VL 30
AR UNSP e020
DI 10.1017/pas.2012.020
PG 54
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 161ZZ
UT WOS:000320235100001
ER
PT J
AU Charlton-Perez, AJ
Baldwin, MP
Birner, T
Black, RX
Butler, AH
Calvo, N
Davis, NA
Gerber, EP
Gillett, N
Hardiman, S
Kim, J
Kruger, K
Lee, YY
Manzini, E
McDaniel, BA
Polvani, L
Reichler, T
Shaw, TA
Sigmond, M
Son, SW
Toohey, M
Wilcox, L
Yoden, S
Christiansen, B
Lott, F
Shindell, D
Yukimoto, S
Watanabe, S
AF Charlton-Perez, Andrew J.
Baldwin, Mark P.
Birner, Thomas
Black, Robert X.
Butler, Amy H.
Calvo, Natalia
Davis, Nicholas A.
Gerber, Edwin P.
Gillett, Nathan
Hardiman, Steven
Kim, Junsu
Krueger, Kirstin
Lee, Yun-Young
Manzini, Elisa
McDaniel, Brent A.
Polvani, Lorenzo
Reichler, Thomas
Shaw, Tiffany A.
Sigmond, Michael
Son, Seok-Woo
Toohey, Matthew
Wilcox, Laura
Yoden, Shigeo
Christiansen, Bo
Lott, Franois
Shindell, Drew
Yukimoto, Seiji
Watanabe, Shingo
TI On the lack of stratospheric dynamical variability in low-top versions
of the CMIP5 models
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
ID TEMPERATURE TRENDS; CLIMATE-CHANGE; PART I; WINTER; CIRCULATION; OZONE;
CONFIGURATION; SIMULATIONS; IMPACT; WELL
AB We describe the main differences in simulations of stratospheric climate and variability by models within the fifth Coupled Model Intercomparison Project (CMIP5) that have a model top above the stratopause and relatively fine stratospheric vertical resolution (high-top), and those that have a model top below the stratopause (low-top). Although the simulation of mean stratospheric climate by the two model ensembles is similar, the low-top model ensemble has very weak stratospheric variability on daily and interannual time scales. The frequency of major sudden stratospheric warming events is strongly underestimated by the low-top models with less than half the frequency of events observed in the reanalysis data and high-top models. The lack of stratospheric variability in the low-top models affects their stratosphere-troposphere coupling, resulting in short-lived anomalies in the Northern Annular Mode, which do not produce long-lasting tropospheric impacts, as seen in observations. The lack of stratospheric variability, however, does not appear to have any impact on the ability of the low-top models to reproduce past stratospheric temperature trends. We find little improvement in the simulation of decadal variability for the high-top models compared to the low-top, which is likely related to the fact that neither ensemble produces a realistic dynamical response to volcanic eruptions. Citation: Charlton-Perez, A. J., et al. (2013), On the lack of stratospheric dynamical variability in low-top versions of the CMIP5 models, J. Geophys. Res. Atmos., 118, 2494-2505, doi:10.1002/jgrd.50125.
C1 [Charlton-Perez, Andrew J.] Univ Reading, Dept Meteorol, Reading, Berks, England.
[Baldwin, Mark P.] Univ Exeter, Coll Engn Math & Phys Sci, Exeter, Devon, England.
[Birner, Thomas; Davis, Nicholas A.] Colorado State Univ, Dept Atmospher Sci, Ft Collins, CO 80523 USA.
[Black, Robert X.; Lee, Yun-Young] Georgia Inst Technol, Sch Earth & Atmospher Sci, Atlanta, GA 30332 USA.
[Butler, Amy H.] Climate Predict Ctr, College Pk, MD USA.
[Calvo, Natalia] Univ Complutense Madrid, Dept Fis Tierra 2, Madrid, Spain.
[Gerber, Edwin P.] NYU, New York, NY USA.
[Gillett, Nathan] Canadian Ctr Climate Modelling & Anal, Victoria, BC, Canada.
[Hardiman, Steven] Met Off, Exeter, Devon, England.
[Kim, Junsu; Reichler, Thomas] Univ Utah, Dept Atmospher Sci, Salt Lake City, UT 84112 USA.
[Manzini, Elisa] Max Planck Inst Meteorol, D-20146 Hamburg, Germany.
[McDaniel, Brent A.] Kennesaw State Univ, Dept Biol & Phys, Kennesaw, GA USA.
[Polvani, Lorenzo; Shaw, Tiffany A.] Columbia Univ, Dept Appl Math & Appl Phys, New York, NY USA.
[Sigmond, Michael] Univ Toronto, Dept Phys, Toronto, ON, Canada.
[Son, Seok-Woo] Seoul Natl Univ, Sch Earth & Environm Sci, Seoul 151, South Korea.
[Krueger, Kirstin; Toohey, Matthew] GEOMAR Helmholtz Ctr Ocean Res Kiel, Kiel, Germany.
[Wilcox, Laura] Univ Reading, Natl Ctr Atmospher Sci, Reading, Berks, England.
[Yoden, Shigeo] Kyoto Univ, Kyoto, Japan.
[Christiansen, Bo] Danish Meteorol Inst, Copenhagen, Denmark.
[Lott, Franois] Ecole Normale Super, Lab Meteorol Dynam, F-75231 Paris, France.
[Shindell, Drew] NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
[Yukimoto, Seiji] Met Res Inst, Tsukuba, Ibaraki, Japan.
[Watanabe, Shingo] JAMSTEC, Res Inst Global Change, Tokyo, Japan.
RP Charlton-Perez, AJ (reprint author), Univ Reading, Dept Meteorol, Reading, Berks, England.
EM a.j.charlton@reading.ac.uk
RI Sigmond, Michael /K-3169-2012; Wilcox, Laura/F-3394-2013; Toohey,
Matthew/G-3129-2010; Butler, Amy/K-6190-2012; Birner,
Thomas/A-2108-2008; Shindell, Drew/D-4636-2012; Son, Seok-Woo
/A-8797-2013; YODEN, SHIGEO/P-9065-2014; Black, Robert/L-8522-2014;
Watanabe, Shingo/L-9689-2014;
OI Christiansen, Bo/0000-0003-2792-4724; Charlton-Perez,
Andrew/0000-0001-8179-6220; Sigmond, Michael /0000-0003-2191-9756;
Wilcox, Laura/0000-0001-5691-1493; Toohey, Matthew/0000-0002-7070-405X;
Butler, Amy/0000-0002-3632-0925; Birner, Thomas/0000-0002-2966-3428;
Watanabe, Shingo/0000-0002-2228-0088; CALVO FERNANDEZ,
NATALIA/0000-0001-6213-1864
FU National Centre for Atmospheric Science [CMIP5]; NSF under the US CLIVAR
program; NSF under Office of Polar Program; U.S. National Science
Foundation; U.S. Department of Energy, Office of Biological and
Environmental Research [DE-FOA000024]; National Science Foundation
[ARC-1107384]; Spanish Ministry of Science and Innovation (MCINN)
[CGL2008-05968-C02-01]; National Science Foundation; BMBF [01LP1130B];
Joint DECC/Defra Met Office Hadley Centre Climate Programme [GA01101];
European Commission [226520]
FX We acknowledge the World Climate Research Programme's Working Group on
Coupled Modelling, which is responsible for CMIP, and we thank the
climate modeling groups for producing and making available the model
output listed in Table 1. For CMIP the U.S. Department of Energy's
Program for Climate Model Diagnosis and Intercomparison provides
coordinating support and led development of software infrastructure in
partnership with the Global Organization for Earth System Science
Portals. A. J. C.-P. and L. J. W. were supported by an National Centre
for Atmospheric Science CMIP5 grant. M. P. B. was funded by NSF under
the US CLIVAR program and the Office of Polar Programs. T. B. and N. A.
D. acknowledge support by the U.S. National Science Foundation. The
research efforts of R. X. B., B. A. M. & Y.-Y. L. were conducted under
support by the U.S. Department of Energy, Office of Biological and
Environmental Research, Award No. DE-FOA000024 and by the National
Science Foundation Grant, ARC-1107384. N. C. was supported by the
Spanish Ministry of Science and Innovation (MCINN) through the
CGL2008-05968-C02-01 project. E. P. G. was supported by the National
Science Foundation. The work of M. T. and K. K. contributes to the BMBF
joint research project MiKlip within the project ALARM through the grant
01LP1130B. The work of S. C. H. was supported by the Joint DECC/Defra
Met Office Hadley Centre Climate Programme (GA01101). We also
acknowledge the European Commission's 7th Framework Programme, under
Grant Agreement number 226520, COMBINE project which supplied some data
not available from the CMIP5 archive. We also thank Gerard Devine
(NCAS-CMS) for help with accessing and parsing meta-data information
from the models.
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PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-897X
EI 2169-8996
J9 J GEOPHYS RES-ATMOS
JI J. Geophys. Res.-Atmos.
PD MAR 27
PY 2013
VL 118
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BP 2494
EP 2505
DI 10.1002/jgrd.50125
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WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 129MB
UT WOS:000317843200003
ER
PT J
AU Bergman, JW
Fierli, F
Jensen, EJ
Honomichl, S
Pan, LL
AF Bergman, John W.
Fierli, Federico
Jensen, Eric J.
Honomichl, Shawn
Pan, Laura L.
TI Boundary layer sources for the Asian anticyclone: Regional contributions
to a vertical conduit
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
ID TROPICAL TROPOPAUSE LAYER; LOWER STRATOSPHERE; SUMMER MONSOON;
WATER-VAPOR; SEASONAL-VARIATION; TRANSPORT; MODEL; AIR; TRAJECTORIES;
CIRCULATION
AB The transport of air from the planetary boundary layer (PBL) into the Asian Summer Monsoon anticyclone is investigated using backward trajectories initiated within the anti-cyclone at 100 mb and 200 mb during August 2011. Transport occurs through a well-defined conduit centered over the southern Tibetan plateau, where convection lofts air parcels into the anticyclone. The conduit, as a dynamical feature, is distinct from the anticyclone. Thus, while the anticyclone influences transport through the upper troposphere and lower stratosphere, it does not by itself define a transport pipeline through that region. To quantify model sensitivities, parcel trajectories are calculated using wind fields from multiple analysis data sets (European Centre for Medium-Range Weather Forecasts, National Center for Environmental Prediction's Global Forecasting System, and NASA's Modern-Era Retrospective Analysis for Research and Applications [MERRA]) and from synthetically modified data sets that explore the roles of vertical motion and horizontal resolution for discrepancies among these calculations. All calculations agree on the relative contributions to PBL sources for the anticyclone from large-scale regions with Tibetan Plateau and India/SE Asia being the most important. However, they disagree on the total fraction of air within the anticyclone that was recently in the PBL. At 200 mbar, calculations using MERRA are clear outliers due to problematic vertical motion in those data. Large differences among the different data sets at 100 mbar are more closely related to horizontal resolution. It is speculated that this reflects the importance of deep, small-scale convective updrafts for transport to 100 mbar. Citation: Bergman, J. W., F. Fierli, E. J. Jensen, S. Honomichl, and L. L. Pan (2013), Boundary layer sources for the Asian anticyclone: Regional contributions to a vertical conduit, J. Geophys. Res. Atmos., 118, 2560-2575, doi:10.1002/jgrd.50142.
C1 [Bergman, John W.] Bay Area Environm Res Inst, Sonoma, CA USA.
[Bergman, John W.; Honomichl, Shawn; Pan, Laura L.] Natl Ctr Atmospher Res, Div Atmospher Chem, Boulder, CO 80307 USA.
[Fierli, Federico] CNR, Inst Atmospher Sci & Climate, Rome, Italy.
[Jensen, Eric J.] NASA, Ames Res Ctr, Div Earth Sci, Moffett Field, CA 94035 USA.
RP Bergman, JW (reprint author), Natl Ctr Atmospher Res, Div Atmospher Chem, POB 3000, Boulder, CO 80307 USA.
EM bergman@ucar.edu
RI Pan, Laura/A-9296-2008;
OI Pan, Laura/0000-0001-7377-2114; Fierli, Federico/0000-0001-9975-2883
FU National Science Foundation
FX This work benefitted from helpful conversations with and comments on
early versions of the manuscript from C. Homeyer, S. Fueglistaler, H.
Garny, M. Park, L. Pfister, W. Randel, and two anonymous reviewers. J.
Bergman. F. Fierli, and E. Jensen were visitors at the Atmospheric
Chemistry Division of NCAR during the execution of this study. The
National Center for Atmospheric Research is operated by the University
Corporation for Atmospheric Research, under sponsorship of the National
Science Foundation.
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PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-897X
EI 2169-8996
J9 J GEOPHYS RES-ATMOS
JI J. Geophys. Res.-Atmos.
PD MAR 27
PY 2013
VL 118
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BP 2560
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SC Meteorology & Atmospheric Sciences
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UT WOS:000317843200008
ER
PT J
AU Allen, DR
Douglass, AR
Strahan, SE
AF Allen, Douglas R.
Douglass, Anne R.
Strahan, Susan E.
TI The large-scale frozen-in anticyclone in the 2011 Arctic summer
stratosphere
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
ID NORTHERN-HEMISPHERE; TRANSPORT MODEL; GMI CHEMISTRY; OZONE LOSS;
CLIMATOLOGY; VORTEX
AB The 2011 Arctic stratospheric final warming was characterized by a large-scale frozen-in anticyclone (FrIAC) that rapidly displaced the winter polar vortex, establishing unusually strong polar easterlies. A comprehensive overview of the 2011 FrIAC is provided using meteorological analyses, Microwave Limb Sounder (MLS) N2O observations, and N2O simulations from the Global Modeling Initiative (GMI) 3-D chemistry and transport model and the Van Leer Icosahedral Triangular Advection (VITA) 2-D (latitude x longitude) isentropic transport model. A vortex edge diagnostic is used to determine the FrIAC boundary, allowing quantification of several FrIAC properties. The 2011 FrIAC originated over North Africa in late March and traveled eastward and poleward over 2 weeks, forming a strong anticyclone that extended from similar to 580-2100 K potential temperature (similar to 25-50 km). Low potential vorticity (PV) was transported to the pole with the FrIAC in early April; during May, most of the PV signature decayed due to diabatic processes. A small remnant negative PV anomaly persisted near the pole until mid-June. Tracer equivalent latitude was low initially and remained low throughout the summer. GMI, VITA, and MLS showed elevated N2O in the FrIAC, although the peak value was smaller in GMI due to a subtropical low bias. The high-resolution (similar to 20 km) VITA filamentary structure quantitatively matched most of the features observed by MLS when smoothed to match the MLS resolution. The high-N2O anomaly persisted in the middle stratosphere over 4 months until late August, when it was destroyed by horizontal and vertical shearing, combined with photochemical processes. Citation: Allen, D. R., A. R. Douglass, and S. E. Strahan (2013), The large-scale frozen-in anticyclone in the 2011 Arctic summer stratosphere, J. Geophys. Res. Atmos., 118, 2656-2672, doi:10.1002/jgrd.50256.
C1 [Allen, Douglas R.] USN, Res Lab, Remote Sensing Div, Washington, DC 20375 USA.
[Douglass, Anne R.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Strahan, Susan E.] Univ Space Res Assoc, Columbia, MD USA.
RP Allen, DR (reprint author), USN, Res Lab, Remote Sensing Div, Washington, DC 20375 USA.
EM Douglas.Allen@nrl.navy.mil
RI Douglass, Anne/D-4655-2012
FU NASA Atmospheric Composition: Modeling and Analysis Program
[NNHH09ZDA001N]; Office of Naval Research
FX This work was supported by a subcontract from the NASA Atmospheric
Composition: Modeling and Analysis Program, NNHH09ZDA001N. Work at the
Naval Research Laboratory is sponsored by the Office of Naval Research.
We would like to thank Gloria Manney for providing the gridded MLS data
used to initialize the VITA simulations. We also acknowledge the Global
Modeling and Assimilation Office and the Goddard Earth Science Data and
Information Services Center for the dissemination of MERRA products.
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SN 2169-897X
J9 J GEOPHYS RES-ATMOS
JI J. Geophys. Res.-Atmos.
PD MAR 27
PY 2013
VL 118
IS 6
BP 2656
EP 2672
DI 10.1002/jgrd.50256
PG 17
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 129MB
UT WOS:000317843200016
ER
PT J
AU Brakebusch, M
Randall, CE
Kinnison, DE
Tilmes, S
Santee, ML
Manney, GL
AF Brakebusch, M.
Randall, C. E.
Kinnison, D. E.
Tilmes, S.
Santee, M. L.
Manney, G. L.
TI Evaluation of Whole Atmosphere Community Climate Model simulations of
ozone during Arctic winter 2004-2005
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
ID POLAR STRATOSPHERIC CLOUD; CHEMICAL-TRANSPORT MODEL; GENERAL-CIRCULATION
MODEL; CHLORINE ACTIVATION; SATELLITE-OBSERVATIONS; 3-DIMENSIONAL MODEL;
DEPLETION; TRACERS; DENITRIFICATION; LATITUDES
AB The work presented here evaluates polar stratospheric ozone simulations from the Whole Atmosphere Community Climate Model (WACCM) for the Arctic winter of 2004-2005. We use the Specified Dynamics version of WACCM (SD-WACCM), in which temperatures and winds are nudged to meteorological assimilation analysis results. Model simulations of ozone and related constituents generally compare well to observations from the Earth Observing System Microwave Limb Sounder (MLS). At most times, modeled ozone agrees with MLS data to within similar to 10%. However, a systematic high bias in ozone in the model of similar to 18% is found in the lowermost stratosphere in March. We attribute most of this ozone bias to too little heterogeneous processing of halogens late in the winter. We suggest that the model under-predicts ClONO2 early in the winter, which leads to less heterogeneous processing and too little activated chlorine. Model HCl could also be overestimated due to an underestimation of HCl uptake into supercooled ternary solution (STS) particles. In late winter, the model overestimates gas-phase HNO3, and thus NOy, which leads to an over-prediction of ClONO2 (under-prediction of activated chlorine). A sensitivity study, in which temperatures for heterogeneous chemistry reactions were reduced by 1.5 K, shows significant improvement of modeled ozone. Chemical ozone loss is inferred from the MLS observations using the pseudo-passive subtraction approach. The inferred ozone loss using this method is in agreement with or less than previous independent results for the Arctic winter of 2004-2005, reaching 1.0 ppmv on average and up to 1.6 ppmv locally in the polar vortex. Citation: Brakebusch, M., C. E. Randall, D. E. Kinnison, S. Tilmes, M. L. Santee, and G. L. Manney (2013), Evaluation of Whole Atmosphere Community Climate Model simulations of ozone during Arctic winter 2004-2005, J. Geophys. Res. Atmos., 118, 2673-2688, doi:10.1002/jgrd.50226.
C1 [Brakebusch, M.; Randall, C. E.] Univ Colorado, Dept Atmospher & Ocean Sci, Boulder, CO 80309 USA.
[Brakebusch, M.; Randall, C. E.] Univ Colorado, Atmospher & Space Phys Lab, Boulder, CO 80309 USA.
[Kinnison, D. E.; Tilmes, S.] Natl Ctr Atmospher Res, Div Atmospher Chem, Boulder, CO 80307 USA.
[Santee, M. L.; Manney, G. L.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Manney, G. L.] New Mexico Inst Min & Technol, Socorro, NM 87801 USA.
RP Brakebusch, M (reprint author), Univ Colorado, Dept Atmospher & Ocean Sci, Boulder, CO 80309 USA.
EM brakebusch@colorado.edu
RI Randall, Cora/L-8760-2014
OI Randall, Cora/0000-0002-4313-4397
FU JPL/NASA grant [1350080]; NSF [AGS 1135432]; National Science
Foundation; National Aeronautics and Space Administration
FX We thank C. S. Singleton for helpful discussions. M. B. and C. E. R.
were funded by JPL/NASA grant 1350080 and NSF award AGS 1135432. The
SD-WACCM simulations were carried out at NCAR. NCAR is sponsored by the
National Science Foundation. Work at the Jet Propulsion Laboratory,
California Institute of Technology, was done under contract with the
National Aeronautics and Space Administration.
NR 67
TC 19
Z9 20
U1 2
U2 30
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-897X
EI 2169-8996
J9 J GEOPHYS RES-ATMOS
JI J. Geophys. Res.-Atmos.
PD MAR 27
PY 2013
VL 118
IS 6
BP 2673
EP 2688
DI 10.1002/jgrd.50226
PG 16
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 129MB
UT WOS:000317843200017
ER
PT J
AU Ting, DZY
Soibel, A
Khoshakhlagh, A
Nguyen, J
Hoglund, L
Keo, SA
Mumolo, JM
Gunapala, SD
AF Ting, David Z. -Y.
Soibel, Alexander
Khoshakhlagh, Arezou
Nguyen, Jean
Hoeglund, Linda
Keo, Sam A.
Mumolo, Jason M.
Gunapala, Sarath D.
TI Exclusion, extraction, and junction placement effects in the
complementary barrier infrared detector
SO APPLIED PHYSICS LETTERS
LA English
DT Article
ID SUPERLATTICE; DEVICES; PERFORMANCE; HGCDTE
AB We demonstrate a long wavelength type-II superlattice (T2SL) complementary barrier infrared detector (CBIRD) with a double broken-gap junction bottom contact structure designed to reduce material growth demands without diminishing performance. Simulation suggests generation-recombination dark current suppression is the result of placing the electrical junction in the wide-gap hole barrier region, away from the metallurgical hole-barrier/ absorber heterojunction. The lower turn-on bias of the modified CBIRD is explained in terms of junction properties. We suggest that minority carrier exclusion and extraction effects are partially responsible for the observed low diffusion-limited CBIRD dark current despite short T2SL minority carrier lifetimes. (C) 2013 American Institute of Physics. [http://dx.doi.org/10.1063/1.4798551]
C1 [Ting, David Z. -Y.; Soibel, Alexander; Khoshakhlagh, Arezou; Nguyen, Jean; Hoeglund, Linda; Keo, Sam A.; Mumolo, Jason M.; Gunapala, Sarath D.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Ting, DZY (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM David.Z.Ting@jpl.nasa.gov
RI Soibel, Alexander/A-1313-2007
FU National Aeronautics and Space Administration
FX The authors thank S. Bandara, E.S. Daniel, E.R. Blazejewski, T.J.
Cunningham, D.R. Rhiger, R.E. de Wames, and J.N. Schulman for helpful
discussions and R. Liang, M. Herman, E. Kolawa, and M. Tidrow for
encouragement and support. The research described in this publication
was carried out at the Jet Propulsion Laboratory, California Institute
of Technology, under a contract with the National Aeronautics and Space
Administration.
NR 18
TC 12
Z9 12
U1 0
U2 18
PU AMER INST PHYSICS
PI MELVILLE
PA CIRCULATION & FULFILLMENT DIV, 2 HUNTINGTON QUADRANGLE, STE 1 N O 1,
MELVILLE, NY 11747-4501 USA
SN 0003-6951
J9 APPL PHYS LETT
JI Appl. Phys. Lett.
PD MAR 25
PY 2013
VL 102
IS 12
AR 121109
DI 10.1063/1.4798551
PG 4
WC Physics, Applied
SC Physics
GA 117QB
UT WOS:000316967100009
ER
PT J
AU Dietz, A
Fotopoulos, N
Singer, L
Cutler, C
AF Dietz, Alexander
Fotopoulos, Nickolas
Singer, Leo
Cutler, Curt
TI Outlook for detection of GW inspirals by GRB-triggered searches in the
advanced detector era
SO PHYSICAL REVIEW D
LA English
DT Article
ID GAMMA-RAY BURSTS; GRAVITATIONAL-WAVES; LIGO OBSERVATIONS; COMPACT
BINARIES; SCIENCE RUN; JET BREAKS; TELESCOPE; AFTERGLOW; DURATION;
ORIGIN
AB Short, hard gamma-ray bursts (GRBs) are believed to originate from the coalescence of two neutron stars (NSs) or a NS and a black hole (BH). If this scenario is correct, then short GRBs will be accompanied by the emission of strong gravitational waves (GWs), detectable by GW observatories such as LIGO, Virgo, KAGRA, and LIGO-India. As compared with blind, all-sky, all-time GW searches, externally triggered searches for GW counterparts to short GRBs have the advantages of both significantly reduced detection threshold due to known time and sky location and enhanced GW amplitude because of face-on orientation. Based on the distribution of signal-to-noise ratios in candidate compact binary coalescence events in the most recent joint LIGO-Virgo data, our analytic estimates, and our Monte Carlo simulations, we find an effective sensitive volume for GRB-triggered searches that is approximate to 2 times greater than for an all-sky, all-time search. For NS-NS systems, a jet angle theta(j) = 20 degrees, a gamma-ray satellite field of view of 10% of the sky, and priors with generally precessing spin, this doubles the number of NS-NS short-GRB and NS-BH short-GRB associations, to similar to 3-4% of all detections of NS-NSs and NS-BHs. We also investigate the power of tests for statistical excesses in lists of subthreshold events, and show that these are unlikely to reveal a subthreshold population until finding GW associations to short GRBs is already routine. Finally, we provide useful formulas for calculating the prior distribution of GW amplitudes from a compact binary coalescence, for a given GW detector network and given sky location. DOI: 10.1103/PhysRevD.87.064033
C1 [Dietz, Alexander] Univ Mississippi, Dept Phys & Astron, University, MS 38677 USA.
[Fotopoulos, Nickolas; Singer, Leo] CALTECH, LIGO Lab, Pasadena, CA 91125 USA.
[Cutler, Curt] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Dietz, A (reprint author), Univ Mississippi, Dept Phys & Astron, University, MS 38677 USA.
FU National Science Foundation (NSF) [PHY-0107417]; NSF; NSF [PHY-1067985,
PHY-0757937, PHY1068881]; National Aeronautics and Space Administration
FX The authors thank Alan Weinstein and Michal Was for comments on the
manuscript, and Neil Gehrels for updating us on GRB missions. LIGO was
constructed by the California Institute of Technology and Massachusetts
Institute of Technology with funding from the National Science
Foundation (NSF) and operates under cooperative agreement No.
PHY-0107417. L. S. is supported by the NSF through a Graduate Research
Fellowship, while A. D. is supported by NSF Grants No. PHY-1067985 and
No. PHY-0757937. C. C.'s work was carried out at the Jet Propulsion
Laboratory, California Institute of Technology, under contract to the
National Aeronautics and Space Administration. C. C. also gratefully
acknowledges support from NSF Grant No. PHY1068881. This paper has LIGO
Document No. LIGO-P1200113- v7.
NR 55
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U1 0
U2 7
PU AMER PHYSICAL SOC
PI COLLEGE PK
PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA
SN 1550-7998
J9 PHYS REV D
JI Phys. Rev. D
PD MAR 22
PY 2013
VL 87
IS 6
AR 064033
DI 10.1103/PhysRevD.87.064033
PG 13
WC Astronomy & Astrophysics; Physics, Particles & Fields
SC Astronomy & Astrophysics; Physics
GA 113NZ
UT WOS:000316676000006
ER
PT J
AU Marley, MS
AF Marley, Mark S.
TI Probing an Extrasolar Planet
SO SCIENCE
LA English
DT Editorial Material
ID ORBITING HR 8799; MU-M; ATMOSPHERE; SPECTRUM; ABSORPTION; JUPITER;
CARBON; MASSES; WATER
C1 NASA, Ames Res Ctr, Div Space Sci, Moffett Field, CA 94035 USA.
RP Marley, MS (reprint author), NASA, Ames Res Ctr, Div Space Sci, Moffett Field, CA 94035 USA.
EM mark.s.marley@nasa.gov
RI Marley, Mark/I-4704-2013;
OI Marley, Mark/0000-0002-5251-2943
NR 15
TC 2
Z9 2
U1 0
U2 5
PU AMER ASSOC ADVANCEMENT SCIENCE
PI WASHINGTON
PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 USA
SN 0036-8075
J9 SCIENCE
JI Science
PD MAR 22
PY 2013
VL 339
IS 6126
BP 1393
EP 1394
DI 10.1126/science.1235078
PG 2
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 114KU
UT WOS:000316740700030
PM 23520101
ER
PT J
AU Maphutha, S
Moothi, K
Meyyappan, M
Iyuke, SE
AF Maphutha, Selby
Moothi, Kapil
Meyyappan, M.
Iyuke, Sunny E.
TI A carbon nanotube-infused polysulfone membrane with polyvinyl alcohol
layer for treating oil-containing waste water
SO SCIENTIFIC REPORTS
LA English
DT Article
ID POLY(VINYL ALCOHOL); MECHANICAL-PROPERTIES; POLYMER COMPOSITES;
CROSS-LINKING; ULTRAFILTRATION; MICROFILTRATION; NANOFILTRATION;
PERFORMANCE; EMULSION; REINFORCEMENT
AB A carbon nanotube (CNT) integrated polymer composite membrane with a polyvinyl alcohol barrier layer has been prepared to separate oil from water for treatment of oil-containing waste water. The CNTs were synthesised using chemical vapour deposition, and a phase inversion method was employed for the blending of the CNTs in the polymer composite solution for casting of the membrane. Relative to the baseline polymer, an increase of 119% in the tensile strength, 77% in the Young's modulus and 258% in the toughness is seen for a concentration of 7.5% CNTs in the polymer composite. The permeate through the membrane shows oil concentrations below the acceptable 10 mg/L limit with an excellent throughput and oil rejection of over 95%.
C1 [Maphutha, Selby; Moothi, Kapil; Iyuke, Sunny E.] Univ Witwatersrand, Sch Chem & Met Engn, ZA-2050 Wits, South Africa.
[Maphutha, Selby; Moothi, Kapil; Iyuke, Sunny E.] DST NRF Ctr Excellence Strong Mat, ZA-2050 Wits 2050, South Africa.
[Meyyappan, M.] NASA, Ames Res Ctr, Ctr Nanotechnol, Moffett Field, CA 94035 USA.
[Meyyappan, M.] POSTECH, Div IT Convergence Engn, Pohang, South Korea.
RP Iyuke, SE (reprint author), Univ Witwatersrand, Sch Chem & Met Engn, P Bag 3, ZA-2050 Wits, South Africa.
EM Sunny.Iyuke@wits.ac.za
OI Moothi, Kapil/0000-0001-7755-5125; Maphutha, Selby/0000-0003-3105-9016
FU National Research Foundation (NRF) under South Africa Focus Area; NRF
Nanotechnology flagship programme; Department of Science and Technology
(DST)/NRF Centre of Excellence; World Class University program through
the National Research Foundation of Korea; Ministry of Education,
Science and Technology [R31-10100]
FX The authors acknowledge the financial support from the National Research
Foundation (NRF) under South Africa Focus Area, NRF Nanotechnology
flagship programme, Department of Science and Technology (DST)/NRF
Centre of Excellence. The student bursaries provided by the University
of the Witwatersrand are acknowledged. The work in Korea was supported
by the World Class University program through the National Research
Foundation of Korea funded by the Ministry of Education, Science and
Technology under Project R31-10100.
NR 40
TC 24
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U1 6
U2 74
PU NATURE PUBLISHING GROUP
PI LONDON
PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND
SN 2045-2322
J9 SCI REP-UK
JI Sci Rep
PD MAR 22
PY 2013
VL 3
AR 1509
DI 10.1038/srep01509
PG 6
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 111TO
UT WOS:000316543800001
PM 23518875
ER
PT J
AU Vieira, JD
Marrone, DP
Chapman, SC
De Breuck, C
Hezaveh, YD
Weiss, A
Aguirre, JE
Aird, KA
Aravena, M
Ashby, MLN
Bayliss, M
Benson, BA
Biggs, AD
Bleem, LE
Bock, JJ
Bothwell, M
Bradford, CM
Brodwin, M
Carlstrom, JE
Chang, CL
Crawford, TM
Crites, AT
de Haan, T
Dobbs, MA
Fomalont, EB
Fassnacht, CD
George, EM
Gladders, MD
Gonzalez, AH
Greve, TR
Gullberg, B
Halverson, NW
High, FW
Holder, GP
Holzapfel, WL
Hoover, S
Hrubes, JD
Hunter, TR
Keisler, R
Lee, AT
Leitch, EM
Lueker, M
Luong-Van, D
Malkan, M
McIntyre, V
McMahon, JJ
Mehl, J
Menten, KM
Meyer, SS
Mocanu, LM
Murphy, EJ
Natoli, T
Padin, S
Plagge, T
Reichardt, CL
Rest, A
Ruel, J
Ruhl, JE
Sharon, K
Schaffer, KK
Shaw, L
Shirokoff, E
Spilker, JS
Stalder, B
Staniszewski, Z
Stark, AA
Story, K
Vanderlinde, K
Welikala, N
Williamson, R
AF Vieira, J. D.
Marrone, D. P.
Chapman, S. C.
De Breuck, C.
Hezaveh, Y. D.
Weiss, A.
Aguirre, J. E.
Aird, K. A.
Aravena, M.
Ashby, M. L. N.
Bayliss, M.
Benson, B. A.
Biggs, A. D.
Bleem, L. E.
Bock, J. J.
Bothwell, M.
Bradford, C. M.
Brodwin, M.
Carlstrom, J. E.
Chang, C. L.
Crawford, T. M.
Crites, A. T.
de Haan, T.
Dobbs, M. A.
Fomalont, E. B.
Fassnacht, C. D.
George, E. M.
Gladders, M. D.
Gonzalez, A. H.
Greve, T. R.
Gullberg, B.
Halverson, N. W.
High, F. W.
Holder, G. P.
Holzapfel, W. L.
Hoover, S.
Hrubes, J. D.
Hunter, T. R.
Keisler, R.
Lee, A. T.
Leitch, E. M.
Lueker, M.
Luong-Van, D.
Malkan, M.
McIntyre, V.
McMahon, J. J.
Mehl, J.
Menten, K. M.
Meyer, S. S.
Mocanu, L. M.
Murphy, E. J.
Natoli, T.
Padin, S.
Plagge, T.
Reichardt, C. L.
Rest, A.
Ruel, J.
Ruhl, J. E.
Sharon, K.
Schaffer, K. K.
Shaw, L.
Shirokoff, E.
Spilker, J. S.
Stalder, B.
Staniszewski, Z.
Stark, A. A.
Story, K.
Vanderlinde, K.
Welikala, N.
Williamson, R.
TI Dusty starburst galaxies in the early Universe as revealed by
gravitational lensing
SO NATURE
LA English
DT Article
ID SOUTH-POLE TELESCOPE; SUBMILLIMETER GALAXY; MOLECULAR GAS; DEEP-FIELD;
REDSHIFT; COUNTS; MODEL
AB In the past decade, our understanding of galaxy evolution has been revolutionized by the discovery that luminous, dusty starburst galaxies were 1,000 times more abundant in the early Universe than at present(1,2). It has, however, been difficult to measure the complete redshift distribution of these objects, especially at the highest redshifts (z>4). Here we report a redshift survey at a wavelength of three millimetres, targeting carbon monoxide line emission from the star-forming molecular gas in the direction of extraordinarily bright millimetre-wave-selected sources. High-resolution imaging demonstrates that these sources are strongly gravitationally lensed by foreground galaxies. We detect spectral lines in 23 out of 26 sources and multiple lines in 12 of those 23 sources, from which we obtain robust, unambiguous redshifts. At least 10 of the sources are found to lie at z > 4, indicating that the fraction of dusty starburst galaxies at high redshifts is greater than previously thought. Models of lens geometries in the sample indicate that the background objects are ultra-luminous infrared galaxies, powered by extreme bursts of star formation.
C1 [Vieira, J. D.; Bock, J. J.; Lueker, M.; Padin, S.; Shirokoff, E.; Staniszewski, Z.] CALTECH, Pasadena, CA 91125 USA.
[Marrone, D. P.; Bothwell, M.; Spilker, J. S.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA.
[Chapman, S. C.] Dalhousie Univ, Dept Phys & Atmospher Sci, Halifax, NS B3H 3J5, Canada.
[Chapman, S. C.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England.
[De Breuck, C.; Aravena, M.; Biggs, A. D.; Gullberg, B.] European So Observ, D-85748 Garching, Germany.
[Hezaveh, Y. D.; de Haan, T.; Dobbs, M. A.; Holder, G. P.; Shaw, L.; Vanderlinde, K.] McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada.
[Weiss, A.; Menten, K. M.] Max Planck Inst Radioastron, D-53121 Bonn, Germany.
[Aguirre, J. E.] Univ Penn, Philadelphia, PA 19104 USA.
[Aird, K. A.; Hrubes, J. D.; Luong-Van, D.] Univ Chicago, Chicago, IL 60637 USA.
[Ashby, M. L. N.; Stalder, B.; Stark, A. A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Bayliss, M.; Ruel, J.] Harvard Univ, Dept Phys, Cambridge, MA 02138 USA.
[Benson, B. A.; Bleem, L. E.; Carlstrom, J. E.; Chang, C. L.; Crawford, T. M.; Crites, A. T.; Gladders, M. D.; High, F. W.; Hoover, S.; Keisler, R.; Leitch, E. M.; McMahon, J. J.; Mehl, J.; Meyer, S. S.; Mocanu, L. M.; Natoli, T.; Padin, S.; Plagge, T.; Sharon, K.; Schaffer, K. K.; Story, K.; Williamson, R.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA.
[Benson, B. A.; Carlstrom, J. E.; Chang, C. L.; Hoover, S.; McMahon, J. J.; Meyer, S. S.] Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA.
[Bleem, L. E.; Carlstrom, J. E.; Keisler, R.; Meyer, S. S.; Natoli, T.; Story, K.] Univ Chicago, Dept Phys, Chicago, IL 60637 USA.
[Bock, J. J.; Bradford, C. M.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Brodwin, M.] Univ Missouri, Dept Phys & Astron, Kansas City, MO 64110 USA.
[Carlstrom, J. E.; Crawford, T. M.; Crites, A. T.; Gladders, M. D.; High, F. W.; Leitch, E. M.; Mehl, J.; Meyer, S. S.; Mocanu, L. M.; Padin, S.; Plagge, T.; Sharon, K.; Williamson, R.] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA.
[Carlstrom, J. E.; Chang, C. L.] Argonne Natl Lab, Argonne, IL 60439 USA.
[Fomalont, E. B.; Hunter, T. R.] Natl Radio Astron Observ, Charlottesville, VA 22903 USA.
[Fassnacht, C. D.] Univ Calif Davis, Dept Phys, Davis, CA 95616 USA.
[George, E. M.; Holzapfel, W. L.; Lee, A. T.; Reichardt, C. L.] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA.
[Gonzalez, A. H.] Univ Florida, Dept Astron, Gainesville, FL 32611 USA.
[Greve, T. R.] UCL, Dept Phys & Astron, London WC1E 6BT, England.
[Halverson, N. W.] Univ Colorado, Dept Astrophys & Planetary Sci, Boulder, CO 80309 USA.
[Halverson, N. W.] Univ Colorado, Dept Phys, Boulder, CO 80309 USA.
[Lee, A. T.] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Dept Phys, Berkeley, CA 94720 USA.
[Malkan, M.] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA.
[McIntyre, V.] CSIRO, Australia Telescope Natl Facil, Epping, NSW 1710, Australia.
[McMahon, J. J.] Univ Michigan, Dept Phys, Ann Arbor, MI 48109 USA.
[Murphy, E. J.] Observ Carnegie Inst Sci, Pasadena, CA 91101 USA.
[Rest, A.] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
[Ruhl, J. E.; Staniszewski, Z.] Case Western Reserve Univ, Dept Phys, Ctr Educ & Res Cosmol & Astrophys, Cleveland, OH 44106 USA.
[Sharon, K.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA.
[Schaffer, K. K.] Sch Art Inst Chicago, Liberal Arts Dept, Chicago, IL 60603 USA.
[Shaw, L.] Yale Univ, Dept Phys, New Haven, CT 06520 USA.
[Welikala, N.] Univ Paris 11, Inst Astrophys Spatiale, F-91405 Orsay, France.
[Welikala, N.] CNRS, F-91405 Orsay, France.
RP Vieira, JD (reprint author), CALTECH, 1200 East Calif Blvd, Pasadena, CA 91125 USA.
EM vieira@caltech.edu
RI Holzapfel, William/I-4836-2015; Williamson, Ross/H-1734-2015;
OI Williamson, Ross/0000-0002-6945-2975; Marrone,
Daniel/0000-0002-2367-1080; Aird, Kenneth/0000-0003-1441-9518;
Reichardt, Christian/0000-0003-2226-9169; De Breuck,
Carlos/0000-0002-6637-3315; Hunter, Todd/0000-0001-6492-0090; Stark,
Antony/0000-0002-2718-9996
FU National Science Foundation; Kavli Foundation; Gordon and Betty Moore
Foundation; NASA from the Space Telescope Science Institute; NSERC; CRC;
ClfAR
FX The SPT is supported by the National Science Foundation, the Kavli
Foundation and the Gordon and Betty Moore Foundation. ALMA is a
partnership of ESO (representing its member states), NSF (USA) and NINS
(Japan), together with NRC (Canada) and NSC and ASIAA (Taiwan), in
cooperation with Chile. The Joint ALMA Observatory is operated by ESO,
AUI/NRAO and NAOJ. The National Radio Astronomy Observatory is a
facility of the NSF operated under cooperative agreement by Associated
Universities, Inc. Partial support for this work was provided by NASA
from the Space Telescope Science Institute. This work is based in part
on observations made with Herschel, a European Space Agency Cornerstone
Mission with significant participation by NASA. Work at McGill
University is supported by NSERC, the CRC programme and ClfAR.
NR 27
TC 109
Z9 109
U1 1
U2 16
PU NATURE PUBLISHING GROUP
PI LONDON
PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND
SN 0028-0836
EI 1476-4687
J9 NATURE
JI Nature
PD MAR 21
PY 2013
VL 495
IS 7441
BP 344
EP 347
DI 10.1038/nature12001
PG 4
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 113EY
UT WOS:000316650500037
PM 23485967
ER
PT J
AU Nowicki, SF
Hunter, SD
Parsons, AM
AF Nowicki, Suzanne F.
Hunter, Stanley D.
Parsons, Ann M.
TI Development of a quasi-monoenergetic 6 MeV Gamma Facility at NASA
Goddard Space Flight Center
SO NUCLEAR INSTRUMENTS & METHODS IN PHYSICS RESEARCH SECTION A-ACCELERATORS
SPECTROMETERS DETECTORS AND ASSOCIATED EQUIPMENT
LA English
DT Article
DE 6.129 MeV; Monoenergetic; Facility; Characterization; Calibration;
Gamma-ray; Neutron; Pulsed neutron generator
ID NEUTRON
AB The 6 MeV Gamma Facility has been developed at NASA Goddard Space Flight Center (GSFC) to allow in-house characterization and testing of a wide range of gamma-ray instruments such as pixelated CdZnTe detectors for planetary science and Compton and pair-production imaging telescopes for astrophysics. The 6 MeV Gamma Facility utilizes a circulating flow of water irradiated by 14 MeV neutrons to produce gamma rays via neutron capture on oxygen (O-16(n,p)N-16 -> O-16*-> O-16+gamma) The facility provides a low cost, in-house source of 2.742, 6.129 and 7.117 MeV gamma rays, near the lower energy range of most accelerators and well above the 2.614 MeV line from the Th-228 decay chain, the highest energy gamma ray available from a natural radionuclide. The 7.13 s half-life of the N-16 decay allows the water to be irradiated on one side of a large granite block and pumped to the opposite side to decay. Separating the irradiation and decay regions allows for shielding material, the granite block, to be placed between them, thus reducing the low-energy gamma-ray continuum. Comparison between high purity germanium (HPGe) spectra from the facility and a manufactured source, Pu-238/C-13, shows that the low-energy continuum from the facility is reduced by a factor similar to 30 and the gamma-ray rate is similar to 100 times higher at 6.129 MeV. (C) 2012 Elsevier B.V. All rights reserved.
C1 [Nowicki, Suzanne F.] Univ Space Res Assoc, Columbia, MD 21044 USA.
[Nowicki, Suzanne F.] Univ Michigan, Ann Arbor, MI 48109 USA.
[Nowicki, Suzanne F.; Hunter, Stanley D.; Parsons, Ann M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Nowicki, SF (reprint author), NASA, Goddard Space Flight Ctr, 8800 Greenbelt Rd,Bldg 34,Room W271, Greenbelt, MD 20771 USA.
EM suzanne.f.nowicki@nasa.gov
FU NASA GSFC Internal Research and Development (IRAD); NASA GSFC
neutron/gamma-ray group
FX This work was supported by NASA GSFC Internal Research and Development
(IRAD). The authors would like to thank Bert Nahory for assembling the
facility, Julia Bodnarik and Robert Forsythe for their help during
operations, and Jeffrey Schweitzer and the NASA GSFC neutron/gamma-ray
group for their support throughout this work.
NR 13
TC 2
Z9 2
U1 0
U2 7
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0168-9002
J9 NUCL INSTRUM METH A
JI Nucl. Instrum. Methods Phys. Res. Sect. A-Accel. Spectrom. Dect. Assoc.
Equip.
PD MAR 21
PY 2013
VL 705
BP 111
EP 116
DI 10.1016/j.nima.2012.12.066
PG 6
WC Instruments & Instrumentation; Nuclear Science & Technology; Physics,
Nuclear; Physics, Particles & Fields
SC Instruments & Instrumentation; Nuclear Science & Technology; Physics
GA 088HX
UT WOS:000314826000016
ER
PT J
AU Edelson, R
Mushotzky, R
Vaughan, S
Scargle, J
Gandhi, P
Malkan, M
Baumgartner, W
AF Edelson, R.
Mushotzky, R.
Vaughan, S.
Scargle, J.
Gandhi, P.
Malkan, M.
Baumgartner, W.
TI KEPLER OBSERVATIONS OF RAPID OPTICAL VARIABILITY IN THE BL LACERTAE
OBJECT W2R1926+42
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE BL Lacertae objects: general; BL Lacertae objects: individual
(W2R1926+42); galaxies: active
ID X-RAY BINARIES; ACTIVE GALACTIC NUCLEI; BLACK-HOLE; GALAXIES; JET;
NOISE; CONNECTION; CATALOG; BLAZARS; LONG
AB We present the first Kepler monitoring of a strongly variable BL Lac, W2R1926+42. The light curve covers 181 days with similar to 0.2% errors, 30 minute sampling and >90% duty cycle, showing numerous delta I/I>25% flares over timescales as short as a day. The flux distribution is highly skewed and non-Gaussian. The variability shows a strong rms-flux correlation with the clearest evidence to date for nonlinearity in this relation. We introduce a method to measure periodograms from the discrete autocorrelation function, an approach that may be well-suited to a wide range of Kepler data. The periodogram is not consistent with a simple power-law, but shows a flattening at frequencies below 7 x 10(-5) Hz. Simple models of the power spectrum, such as a broken power law, do not produce acceptable fits, indicating that the Kepler blazar light curve requires more sophisticated mathematical and physical descriptions than currently in use.
C1 [Edelson, R.; Mushotzky, R.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Mushotzky, R.; Baumgartner, W.] NASA, High Energy Astrophys Lab, GSFC, Greenbelt, MD 20771 USA.
[Vaughan, S.] Univ Leicester, Dept Phys & Astron, Xray & Observat Astron Grp, Leicester LE1 7RH, Leics, England.
[Scargle, J.] NASA, Astrobiol & Space Sci Div, Ames Res Ctr, Stanford, CA 94305 USA.
[Gandhi, P.] Japan Aerosp Explorat Agcy, Inst Space & Astronaut Sci, Chuo Ku, Sagamihara, Kanagawa 2525210, Japan.
[Malkan, M.] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA.
RP Edelson, R (reprint author), Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
EM redelson@astro.umd.edu
FU Kepler GO program through NASA [NNX11AC81G, NNX12AC93G, NNX13AC26G];
NASA Applied Information Systems Research Program
FX The authors appreciate the helpful assistance of the Kepler GO office in
scheduling and understanding these observations, as well as the editor
and anonymous referee for a timely and useful review. This research
utilized data from the HEASARC, IRSA, NED, and MAST data archives, and
the NASA Astrophysics Data System Bibliographic Service. R.E. and R.M.
acknowledge support by the Kepler GO program through NASA grants
NNX11AC81G, NNX12AC93G, and NNX13AC26G. J.S. acknowledges Joe Bredekamp
and the NASA Applied Information Systems Research Program for support.
NR 38
TC 20
Z9 20
U1 2
U2 6
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD MAR 20
PY 2013
VL 766
IS 1
AR 16
DI 10.1088/0004-637X/766/1/16
PG 8
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 105GH
UT WOS:000316054000016
ER
PT J
AU Gezari, S
Martin, DC
Forster, K
Neill, JD
Huber, M
Heckman, T
Bianchi, L
Morrissey, P
Neff, SG
Seibert, M
Schiminovich, D
Wyder, TK
Burgett, WS
Chambers, KC
Kaiser, N
Magnier, EA
Price, PA
Tonry, JL
AF Gezari, S.
Martin, D. C.
Forster, K.
Neill, J. D.
Huber, M.
Heckman, T.
Bianchi, L.
Morrissey, P.
Neff, S. G.
Seibert, M.
Schiminovich, D.
Wyder, T. K.
Burgett, W. S.
Chambers, K. C.
Kaiser, N.
Magnier, E. A.
Price, P. A.
Tonry, J. L.
TI THE GALEX TIME DOMAIN SURVEY. I. SELECTION AND CLASSIFICATION OF OVER A
THOUSAND ULTRAVIOLET VARIABLE SOURCES
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE surveys; ultraviolet: general
ID DIGITAL SKY SURVEY; DEEP FIELD-SOUTH; POINT-SOURCE CATALOG; SURVEY
STRIPE 82; SHOCK BREAKOUT; LIGHT CURVES; TIDAL DISRUPTION; COSMOS FIELD;
OPTICAL VARIABILITY; RED SUPERGIANT
AB We present the selection and classification of over a thousand ultraviolet (UV) variable sources discovered in similar to 40 deg(2) of GALEX Time Domain Survey (TDS) NUV images observed with a cadence of 2 days and a baseline of observations of similar to 3 years. The GALEX TDS fields were designed to be in spatial and temporal coordination with the Pan-STARRS1 Medium Deep Survey, which provides deep optical imaging and simultaneous optical transient detections via image differencing. We characterize the GALEX photometric errors empirically as a function of mean magnitude, and select sources that vary at the 5 sigma level in at least one epoch. We measure the statistical properties of the UV variability, including the structure function on timescales of days and years. We report classifications for the GALEX TDS sample using a combination of optical host colors and morphology, UV light curve characteristics, and matches to archival X-ray, and spectroscopy catalogs. We classify 62% of the sources as active galaxies (358 quasars and 305 active galactic nuclei), and 10% as variable stars (including 37 RR Lyrae, 53 M dwarf flare stars, and 2 cataclysmic variables). We detect a large-amplitude tail in the UV variability distribution for M-dwarf flare stars and RR Lyrae, reaching up to vertical bar Delta m vertical bar = 4.6 mag and 2.9 mag, respectively. The mean amplitude of the structure function for quasars on year timescales is five times larger than observed at optical wavelengths. The remaining unclassified sources include UV-bright extragalactic transients, two of which have been spectroscopically confirmed to be a young core-collapse supernova and a flare from the tidal disruption of a star by dormant supermassive black hole. We calculate a surface density for variable sources in the UV with NUV < 23 mag and vertical bar Delta m vertical bar > 0.2 mag of similar to 8.0, 7.7, and 1.8 deg(-2) for quasars, active galactic nuclei, and RR Lyrae stars, respectively. We also calculate a surface density rate in the UV for transient sources, using the effective survey time at the cadence appropriate to each class, of similar to 15 and 52 deg(-2) yr(-1) for M dwarfs and extragalactic transients, respectively.
C1 [Gezari, S.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Martin, D. C.; Forster, K.; Neill, J. D.; Morrissey, P.; Wyder, T. K.] CALTECH, Dept Astron, Pasadena, CA 91125 USA.
[Huber, M.; Burgett, W. S.; Chambers, K. C.; Kaiser, N.; Magnier, E. A.; Tonry, J. L.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA.
[Heckman, T.; Bianchi, L.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA.
[Neff, S. G.] NASA, Lab Astron & Solar Phys, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Seibert, M.] Observ Carnegie Inst Washington, Pasadena, CA 90095 USA.
[Schiminovich, D.] Columbia Univ, Dept Astron, New York, NY 10027 USA.
[Price, P. A.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA.
RP Gezari, S (reprint author), Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
EM suvi@astro.umd.edu
OI Chambers, Kenneth /0000-0001-6965-7789
FU National Aeronautics and Space Administration through the Planetary
Science Division of the NASA Science Mission Directorate [NNX08AR22G]
FX We thank the anonymous referee for their constructive comments which
improved the paper. GALEX (Galaxy Evolution Explorer) is a NASA Small
Explorer, launched in 2003 April. We gratefully acknowledge NASA's
support for construction, operation, and science analysis for the GALEX
mission, developed in cooperation with the Centre National d'Etudes
Spatiales of France and the Korean Ministry of Science and Technology.
The Pan-STARRS1 survey has been made possible through contributions of
the Institute for Astronomy, the University of Hawaii, the Pan-STARRS
Project Office, the Max Planck Society and its participating institutes,
the Max Planck Institute for Astronomy, Heidelberg and the Max Planck
Institute for Extraterrestrial Physics, Garching, The Johns Hopkins
University, Durham University, the University of Edinburgh, Queen's
University Belfast, the Harvard-Smithsonian Center for Astro-physics,
and the Las Cumbres Observatory Global Telescope Network, Incorporated,
the National Central University of Taiwan, and the National Aeronautics
and Space Administration under grant No. NNX08AR22G issued through the
Planetary Science Division of the NASA Science Mission Directorate.
NR 76
TC 22
Z9 22
U1 0
U2 6
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD MAR 20
PY 2013
VL 766
IS 1
AR 60
DI 10.1088/0004-637X/766/1/60
PG 14
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 105GH
UT WOS:000316054000060
ER
PT J
AU Giacintucci, S
Kale, R
Wik, DR
Venturi, T
Markevitch, M
AF Giacintucci, Simona
Kale, Ruta
Wik, Daniel R.
Venturi, Tiziana
Markevitch, Maxim
TI DISCOVERY OF A GIANT RADIO HALO IN A NEW PLANCK GALAXY CLUSTER
PLCKG171.9-40.7
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: clusters: general; galaxies: clusters: individual
(PLCKG171.9-40.7); intergalactic medium; radio continuum: general;
X-rays: galaxies: clusters
ID X-RAY LUMINOSITY; VLA SKY SURVEY; DEEP 1.4 GHZ; XMM-NEWTON;
SUNYAEV-ZELDOVICH; COSMIC-RAYS; PARTICLE-ACCELERATION; RELIC CANDIDATES;
HADRONIC MODELS; SHOCK-WAVES
AB We report the discovery of a giant radio halo in a new, hot, X-ray luminous galaxy cluster recently found by Planck, PLCKG171.9-40.7. The radio halo was found using Giant Metrewave Radio Telescope observations at 235 MHz and 610 MHz, and in the 1.4 GHz data from an NRAO Very Large Array Sky Survey pointing that we have reanalyzed. The diffuse radio emission is coincident with the cluster X-ray emission, and has an extent of similar to 1 Mpc and a radio power of similar to 5 x 10(24) W Hz(-1) at 1.4 GHz. Its integrated radio spectrum has a slope of alpha approximate to 1.8 between 235 MHz and 1.4 GHz, steeper than that of a typical giant halo. The analysis of the archival XMM-Newton X-ray data shows that the cluster is hot (similar to 10 keV) and disturbed, consistent with X-ray-selected clusters hosting radio halos. This is the first giant radio halo discovered in one of the new clusters found by Planck.
C1 [Giacintucci, Simona] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Giacintucci, Simona] Univ Maryland, Joint Space Sci Inst, College Pk, MD 20742 USA.
[Kale, Ruta; Venturi, Tiziana] INAF Ist Radioastron, I-40129 Bologna, Italy.
[Kale, Ruta] Univ Bologna, Dipartimento Fis & Astron, I-40127 Bologna, Italy.
[Wik, Daniel R.; Markevitch, Maxim] NASA, Astrophys Sci Div, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Giacintucci, S (reprint author), Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
EM simona@astro.umd.edu
OI Venturi, Tiziana/0000-0002-8476-6307
FU NASA [PF0-110071]; Chandra X-ray Center (CXC)
FX We are deeply grateful to Rossella Cassano for useful comments and
suggestions, and for providing Figure 6. We thank Kaustuv Basu for
kindly providing Figure 7. We thank the staff of the GMRT for help
during the observations. GMRT is run by the National Centre for Radio
Astrophysics of the Tata Institute of Fundamental Research. The National
Radio Astronomy Observatory is a facility of the National Science
Foundation operated under cooperative agreement by Associated
Universities, Inc. S.G. acknowledges the support of NASA through
Einstein Postdoctoral Fellowship PF0-110071 awarded by the Chandra X-ray
Center (CXC), which is operated by SAO. This research was supported by
an appointment to the NASA Postdoctoral Program at the Goddard Space
Flight Center, administered by Oak Ridge Associated Universities through
a contract with NASA.
NR 62
TC 10
Z9 10
U1 0
U2 2
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD MAR 20
PY 2013
VL 766
IS 1
AR 18
DI 10.1088/0004-637X/766/1/18
PG 9
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 105GH
UT WOS:000316054000018
ER
PT J
AU Gilliland, RL
Marcy, GW
Rowe, JF
Rogers, L
Torres, G
Fressin, F
Lopez, ED
Buchhave, LA
Christensen-Dalsgaard, J
Desert, JM
Henze, CE
Isaacson, H
Jenkins, J
Lissauer, JJ
Chaplin, WJ
Basu, S
Metcalfe, TS
Elsworth, Y
Handberg, R
Hekker, S
Huber, D
Karoff, C
Kjeldsen, H
Lund, MN
Lundkvist, M
Miglio, A
Charbonneau, D
Ford, EB
Fortney, JJ
Haas, MR
Howard, AW
Howell, SB
Ragozzine, D
Thompson, SE
AF Gilliland, Ronald L.
Marcy, Geoffrey W.
Rowe, Jason F.
Rogers, Leslie
Torres, Guillermo
Fressin, Francois
Lopez, Eric D.
Buchhave, Lars A.
Christensen-Dalsgaard, Jorgen
Desert, Jean-Michel
Henze, Christopher E.
Isaacson, Howard
Jenkins, Jonm.
Lissauer, Jack J.
Chaplin, William J.
Basu, Sarbani
Metcalfe, Travis S.
Elsworth, Yvonne
Handberg, Rasmus
Hekker, Saskia
Huber, Daniel
Karoff, Christoffer
Kjeldsen, Hans
Lund, Mikkel N.
Lundkvist, Mia
Miglio, Andrea
Charbonneau, David
Ford, Eric B.
Fortney, Jonathan J.
Haas, Michael R.
Howard, Andrew W.
Howell, Steve B.
Ragozzine, Darin
Thompson, Susan E.
TI KEPLER-68: THREE PLANETS, ONE WITH A DENSITY BETWEEN THAT OF EARTH AND
ICE GIANTS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE planetary systems; stars: fundamental parameters; stars: individual
(Kepler-68, KIC 11295426, 2MASS J19240775+4902249)
ID SOLAR-TYPE STARS; TESTING BLEND SCENARIOS; SPITZER-SPACE-TELESCOPE;
EXOPLANET HD 189733B; FINE GUIDANCE SENSOR; SUN-LIKE STAR; TRANSITING
PLANET; INITIAL CHARACTERISTICS; EXTRASOLAR PLANETS; ASTEROSEISMIC DATA
AB NASA's Kepler Mission has revealed two transiting planets orbiting Kepler-68. Follow-up Doppler measurements have established the mass of the innermost planet and revealed a third Jovian-mass planet orbiting beyond the two transiting planets. Kepler-68b, in a 5.4 day orbit, has M-P = 8.3(-2.4)(+2.2) M-circle plus, R-P = 2.31(-0.09)(+0.06) R-circle plus, and rho(P) = 3.32(-0.98)(+0.86) g cm(-3), giving Kepler-68b a density intermediate between that of the ice giants and Earth. Kepler-68c is Earth-sized, with a radius R-P = 0.953(-0.042)(+0.037) R-circle plus and transits on a 9.6 day orbit; validation of Kepler-68c posed unique challenges. Kepler-68d has an orbital period of 580 +/- 15 days and a minimum mass of M-P sin i = 0.947 +/- 0.035M(J). Power spectra of the Kepler photometry at one minute cadence exhibit a rich and strong set of asteroseismic pulsation modes enabling detailed analysis of the stellar interior. Spectroscopy of the star coupled with asteroseismic modeling of the multiple pulsation modes yield precise measurements of stellar properties, notably T-eff = 5793 +/- 74 K, M-star = 1.079 +/- 0.051 M-circle dot, R-star = 1.243 +/- 0.019 R-circle dot, and rho(star) = 0.7903 +/- 0.0054 g cm(-3), all measured with fractional uncertainties of only a few percent. Models of Kepler-68b suggest that it is likely composed of rock and water, or has a H and He envelope to yield its density similar to 3 g cm(-3).
C1 [Gilliland, Ronald L.] Penn State Univ, Dept Astron, University Pk, PA 16802 USA.
[Gilliland, Ronald L.] Penn State Univ, Ctr Exoplanets & Habitable Worlds, University Pk, PA 16802 USA.
[Marcy, Geoffrey W.; Isaacson, Howard] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA.
[Rowe, Jason F.; Henze, Christopher E.; Lissauer, Jack J.; Huber, Daniel; Haas, Michael R.; Howell, Steve B.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Rogers, Leslie] CALTECH, Pasadena, CA 91125 USA.
[Torres, Guillermo; Fressin, Francois; Desert, Jean-Michel; Charbonneau, David] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Lopez, Eric D.; Fortney, Jonathan J.] Univ Calif Santa Cruz, Santa Cruz, CA 95064 USA.
[Buchhave, Lars A.] Univ Copenhagen, Niels Bohr Inst, DK-2100 Copenhagen, Denmark.
[Christensen-Dalsgaard, Jorgen; Handberg, Rasmus; Karoff, Christoffer; Kjeldsen, Hans; Lund, Mikkel N.; Lundkvist, Mia] Stellar Astrophys Ctr, Dept Phys & Astron, DK-8000 Aarhus C, Denmark.
[Christensen-Dalsgaard, Jorgen] Natl Ctr Atmospher Res, High Altitude Observ, Boulder, CO 80307 USA.
[Jenkins, Jonm.; Thompson, Susan E.] NASA, Ames Res Ctr, SETI Inst, Moffett Field, CA 94035 USA.
[Chaplin, William J.; Elsworth, Yvonne; Miglio, Andrea] Univ Birmingham, Sch Phys & Astron, Birmingham B15 2TT, W Midlands, England.
[Basu, Sarbani] Yale Univ, Dept Astron, New Haven, CT 06511 USA.
[Metcalfe, Travis S.] White Dwarf Res Corp, Boulder, CO 80301 USA.
[Hekker, Saskia] Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1098 XH Amsterdam, Netherlands.
[Ford, Eric B.; Ragozzine, Darin] Univ Florida, Dept Astron, Gainesville, FL 32611 USA.
[Howard, Andrew W.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA.
RP Gilliland, RL (reprint author), Penn State Univ, Dept Astron, 525 Davey Lab, University Pk, PA 16802 USA.
EM gillil@stsci.edu
RI Howard, Andrew/D-4148-2015;
OI Howard, Andrew/0000-0001-8638-0320; Charbonneau,
David/0000-0002-9003-484X; Fortney, Jonathan/0000-0002-9843-4354;
Buchhave, Lars A./0000-0003-1605-5666; Metcalfe,
Travis/0000-0003-4034-0416; Karoff, Christoffer/0000-0003-2009-7965;
Basu, Sarbani/0000-0002-6163-3472; /0000-0001-6545-639X; Lund, Mikkel
Norup/0000-0001-9214-5642; Lundkvist, Mia Sloth/0000-0002-8661-2571;
Handberg, Rasmus/0000-0001-8725-4502
FU NASA's Science Mission Directorate; W.M. Keck Foundation; NASA,
JPL/Caltech; Space Telescope Science Institute [HF-51313.01-A]; NASA
[NAS 5-26555, NNX12AC75G, AST-1105930, NNX09AG09A]; Danish National
Research Foundation; ASTERISK project (ASTERoseismic Investigations with
SONG and Kepler); European Research Council [267864]; NSF [AST-1105930]
FX Funding for this tenth Discovery mission is provided by NASA's Science
Mission Directorate. The many people contributing to the development of
this mission are gratefully acknowledged. We thank Elizabeth Adams, Eric
Agol, Natalie Batalha, William Borucki, Stephen Bryson, William Cochran,
Andrea Dupree, Debra Fischer, and David Monet for discussion and
contributions. The anonymous referee made comments serving to improve
the paper. Some of the data used here were obtained at the W.M. Keck
Observatory, which is operated as a scientific partnership among the
California Institute of Technology, the University of California, and
NASA. The W.M. Keck Foundation provided generous financial support to
the Keck Observatory. This work is also based in part on observations
made with the Spitzer Space Telescope, which is operated by the Jet
Propulsion Laboratory, California Institute of Technology under a
contract with NASA. Partial support for this work was provided by NASA
through an award issued by JPL/Caltech. Support for L.A.R. was provided
through Hubble Fellowship grant No. HF-51313.01-A awarded by the Space
Telescope Science Institute, which is operated by the Association of
Universities for Research in Astronomy, Inc., for NASA under contract
NAS 5-26555. G.T. acknowledges partial support for this work from NASA
grant NNX12AC75G (Kepler Participating Scientist Program). Funding for
the Stellar Astrophysics Centre is provided by The Danish National
Research Foundation. The research is supported by the ASTERISK project
(ASTERoseismic Investigations with SONG and Kepler) funded by the
European Research Council (grant agreement No. 267864). Asteroseismic
analysis was supported in part by White Dwarf Research Corporation
through the Pale Blue Dot project (http://whitedwarf.org/palebluedot).
S.B. acknowledges support from NSF grant AST-1105930. R.L.G. has been
partially supported by NASA co-operative agreement NNX09AG09A.
NR 107
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U1 0
U2 18
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD MAR 20
PY 2013
VL 766
IS 1
AR 40
DI 10.1088/0004-637X/766/1/40
PG 19
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 105GH
UT WOS:000316054000040
ER
PT J
AU Hermes, JJ
Montgomery, MH
Mullally, F
Winget, DE
Bischoff-Kim, A
AF Hermes, J. J.
Montgomery, M. H.
Mullally, Fergal
Winget, D. E.
Bischoff-Kim, A.
TI A NEW TIMESCALE FOR PERIOD CHANGE IN THE PULSATING DA WHITE DWARF WD
0111+0018
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE stars: individual (WD0111+0018); stars: oscillations (including
pulsations); stars: variables: general; white dwarfs
ID CETI INSTABILITY STRIP; WHOLE EARTH TELESCOPE; DIGITAL SKY SURVEY;
ZZ-CETI; EMPIRICAL DETERMINATION; STARS; ASTEROSEISMOLOGY; G117-B15A;
EVOLUTIONARY; CONVECTION
AB We report the most rapid rate of period change measured to date for a pulsating DA (hydrogen atmosphere) white dwarf (WD), observed in the 292.9 s mode of WD0111+0018. The observed period change, faster than 10(-12) s s(-1), exceeds by more than two orders of magnitude the expected rate from cooling alone for this class of slow and simply evolving pulsating WDs. This result indicates the presence of an additional timescale for period evolution in these pulsating objects. We also measure the rates of period change of nonlinear combination frequencies and show that they share the evolutionary characteristics of their parent modes, confirming that these combination frequencies are not independent modes but rather artifacts of some nonlinear distortion in the outer layers of the star.
C1 [Hermes, J. J.; Montgomery, M. H.; Winget, D. E.] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA.
[Hermes, J. J.; Montgomery, M. H.; Winget, D. E.] McDonald Observ, Ft Davis, TX 79734 USA.
[Mullally, Fergal] SETI Inst, Mountain View, CA 94043 USA.
[Mullally, Fergal] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Bischoff-Kim, A.] Georgia Coll & State Univ, Chem Phys & Astron Dept, Milledgeville, GA 31061 USA.
RP Hermes, JJ (reprint author), Univ Texas Austin, Dept Astron, RLM 15308, Austin, TX 78712 USA.
EM jjhermes@astro.as.utexas.edu
FU Norman Hackerman Advanced Research Program [003658-0255-2007,
003658-0252-2009]; NASA Origins Program [NAG5-13094]; National Science
Foundation [AST-0909107]
FX We are especially grateful to all those whose time in West Texas made
this result possible: S. E. Thompson, C. M. Yeates, K. I. Winget, Davis
Winget, R. E. Nather, Elizabeth J. Jeffery, Ross E. Falcon, and G. F.
Miller. We thank E. L. Robinson, Anjum S. Mukadam, Denis Sullivan, and
Ross E. Falcon for helpful discussions, and acknowledge the McDonald
Observatory staff for tireless support, especially Dave Doss and John
Kuehne. This work is supported by the Norman Hackerman Advanced Research
Program, under grants 003658-0255-2007 and 003658-0252-2009, by a grant
from the NASA Origins Program, NAG5-13094, and by the National Science
Foundation, under grant AST-0909107.
NR 50
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PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD MAR 20
PY 2013
VL 766
IS 1
AR 42
DI 10.1088/0004-637X/766/1/42
PG 9
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 105GH
UT WOS:000316054000042
ER
PT J
AU Houde, M
Fletcher, A
Beck, R
Hildebrand, RH
Vaillancourt, JE
Stil, JM
AF Houde, Martin
Fletcher, Andrew
Beck, Rainer
Hildebrand, Roger H.
Vaillancourt, John E.
Stil, Jeroen M.
TI CHARACTERIZING MAGNETIZED TURBULENCE IN M51
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: individual (M51); galaxies: ISM; galaxies: magnetic fields;
galaxies: spiral
ID COMPRESSIBLE MAGNETOHYDRODYNAMIC TURBULENCE; FIELDS; POLARIZATION;
DISPERSION; ANISOTROPY; GALAXY
AB We use previously published high-resolution synchrotron polarization data to perform an angular dispersion analysis with the aim of characterizing magnetized turbulence in M51. We first analyze three distinct regions (the center of the galaxy, and the northwest and southwest spiral arms) and can clearly discern the turbulent correlation length scale from the width of the magnetized turbulent correlation function for two regions and detect the imprint of anisotropy in the turbulence for all three. Furthermore, analyzing the galaxy as a whole allows us to determine a two-dimensional Gaussian model for the magnetized turbulence in M51. We measure the turbulent correlation scales parallel and perpendicular to the local mean magnetic field to be, respectively, delta(parallel to) = 98 +/- 5 pc and delta(perpendicular to) = 54 +/- 3 pc, while the turbulent-to-ordered magnetic field strength ratio is found to be B-t/B-0 = 1.01 +/- 0.04. These results are consistent with those of Fletcher et al., who performed a Faraday rotation dispersion analysis of the same data, and our detection of anisotropy is consistent with current magnetized turbulence theories.
C1 [Houde, Martin] Univ Western Ontario, Dept Phys & Astron, London, ON N6A 3K7, Canada.
[Houde, Martin] CALTECH, Div Phys Math & Astron, Pasadena, CA 91125 USA.
[Fletcher, Andrew] Newcastle Univ, Sch Math & Stat, Newcastle Upon Tyne NE1 7RU, Tyne & Wear, England.
[Beck, Rainer] Max Planck Inst Radioastron, D-53121 Bonn, Germany.
[Hildebrand, Roger H.] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA.
[Hildebrand, Roger H.] Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA.
[Hildebrand, Roger H.] Univ Chicago, Dept Phys, Chicago, IL 60637 USA.
[Vaillancourt, John E.] NASA, Ames Res Ctr, Stratospher Observ Infrared Astron, Univ Space Res Assoc, Moffett Field, CA 94035 USA.
[Stil, Jeroen M.] Univ Calgary, Dept Phys & Astron, Calgary, AB T2N 1N4, Canada.
RP Houde, M (reprint author), Univ Western Ontario, Dept Phys & Astron, London, ON N6A 3K7, Canada.
FU NSERC Discovery Grant; Canada Research Chair; Western's Academic
Development Fund programs
FX M.H.'s research is funded through the NSERC Discovery Grant, Canada
Research Chair, and Western's Academic Development Fund programs.
NR 21
TC 13
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U1 0
U2 4
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD MAR 20
PY 2013
VL 766
IS 1
AR 49
DI 10.1088/0004-637X/766/1/49
PG 14
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 105GH
UT WOS:000316054000049
ER
PT J
AU Kane, SR
AF Kane, Stephen R.
TI COMPLETENESS OF IMAGING SURVEYS FOR ECCENTRIC EXOPLANETS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE planetary systems; techniques: high angular resolution; techniques:
radial velocities
ID KEPLER PLANET CANDIDATES; RADIAL-VELOCITY SURVEYS; EXTRASOLAR PLANETS;
HR 8799; GIANT PLANETS; ADAPTIVE OPTICS; BETA-PICTORIS; SPECKLE NOISE;
DISK; CONSTRAINTS
AB The detection of exoplanets through direct imaging has produced numerous new positive identifications in recent years. The technique is biased toward planets at wide separations due to the difficulty in removing the stellar signature at small angular separations. Planets in eccentric orbits will thus move in and out of the detectable region around a star as a function of time. Here we use the known diversity of orbital eccentricities to determine the range of orbits that may lie beneath the detection threshold of current surveys. We quantify the percentage of the orbit that yields a detectable signature as a function of semimajor axis, eccentricity, and orbital inclination and estimate the fraction of planets which likely remain hidden by the flux of the host star.
C1 CALTECH, NASA, Exoplanet Sci Inst, Pasadena, CA 91125 USA.
RP Kane, SR (reprint author), CALTECH, NASA, Exoplanet Sci Inst, MS 100-22,770 South Wilson Ave, Pasadena, CA 91125 USA.
EM skane@ipac.caltech.edu
FU National Aeronautics and Space Administration
FX The author thanks Thayne Currie for several enlightening discussions on
this topic, and also Natalie Hinkel for providing useful feedback on the
manuscript. Thanks are also due to the anonymous referee, whose comments
improved the quality of the paper. This research has made use of the
Exoplanet Orbit Database and the Exoplanet Data Explorer at
exoplanets.org. This research has also made use of the NASA Exoplanet
Archive, which is operated by the California Institute of Technology,
under contract with the National Aeronautics and Space Administration
under the Exoplanet Exploration Program.
NR 42
TC 2
Z9 2
U1 0
U2 3
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD MAR 20
PY 2013
VL 766
IS 1
AR 10
DI 10.1088/0004-637X/766/1/10
PG 5
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 105GH
UT WOS:000316054000010
ER
PT J
AU Kwon, RY
Ofman, L
Olmedo, O
Kramar, M
Davila, JM
Thompson, BJ
Cho, KS
AF Kwon, Ryun-Young
Ofman, Leon
Olmedo, Oscar
Kramar, Maxim
Davila, Joseph M.
Thompson, Barbara J.
Cho, Kyung-Suk
TI STEREO OBSERVATIONS OF FAST MAGNETOSONIC WAVES IN THE EXTENDED SOLAR
CORONA ASSOCIATED WITH EIT/EUV WAVES
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE Sun: activity; Sun: corona; Sun: coronal mass ejections (CMEs); Sun:
flares; waves
ID EXTREME-ULTRAVIOLET WAVE; GLOBAL EUV WAVE; LOOP OSCILLATIONS; MASS
EJECTION; EIT WAVES; ACTIVE REGIONS; SHOCK-WAVES; IMAGING TELESCOPE;
TRANSITION-REGION; TRANSIENT WAVES
AB We report white-light observations of a fast magnetosonic wave associated with a coronal mass ejection observed by STEREO/SECCHI/COR1 inner coronagraphs on 2011 August 4. The wave front is observed in the form of density compression passing through various coronal regions such as quiet/active corona, coronal holes, and streamers. Together with measured electron densities determined with STEREO COR1 and Extreme UltraViolet Imager (EUVI) data, we use our kinematic measurements of the wave front to calculate coronal magnetic fields and find that the measured speeds are consistent with characteristic fast magnetosonic speeds in the corona. In addition, the wave front turns out to be the upper coronal counterpart of the EIT wave observed by STEREO EUVI traveling against the solar coronal disk; moreover, stationary fronts of the EIT wave are found to be located at the footpoints of deflected streamers and boundaries of coronal holes, after the wave front in the upper solar corona passes through open magnetic field lines in the streamers. Our findings suggest that the observed EIT wave should be in fact a fast magnetosonic shock/wave traveling in the inhomogeneous solar corona, as part of the fast magnetosonic wave propagating in the extended solar corona.
C1 [Kwon, Ryun-Young] Catholic Univ Amer, Greenbelt, MD 20771 USA.
[Kwon, Ryun-Young; Ofman, Leon; Kramar, Maxim; Davila, Joseph M.; Thompson, Barbara J.; Cho, Kyung-Suk] NASA, Goddard Space Flight Ctr, Solar Phys Lab, Greenbelt, MD 20771 USA.
[Kwon, Ryun-Young; Ofman, Leon; Kramar, Maxim] Catholic Univ Amer, Dept Phys, Inst Astrophys & Computat Sci, Washington, DC 20064 USA.
[Cho, Kyung-Suk] Korea Astron & Space Sci Inst, Taejon 305348, South Korea.
RP Kwon, RY (reprint author), Catholic Univ Amer, Code 671, Greenbelt, MD 20771 USA.
EM ryunyoung.kwon@nasa.gov
RI Thompson, Barbara/C-9429-2012
FU NASA [NNX10AN10G, NNX09AG10G, NNX11AO68G]
FX We are grateful to the referee for a number of constructive comments
that helped to improve the manuscript. R.-Y.K. and L.O. acknowledge
support by NASA grant NNX10AN10G. L.O. also acknowledges support by NASA
grants NNX09AG10G and NNX11AO68G.
NR 69
TC 14
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U1 0
U2 6
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD MAR 20
PY 2013
VL 766
IS 1
AR 55
DI 10.1088/0004-637X/766/1/55
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 105GH
UT WOS:000316054000055
ER
PT J
AU Lindsay, SS
Wooden, DH
Harker, DE
Kelley, MS
Woodward, CE
Murphy, JR
AF Lindsay, Sean S.
Wooden, Diane H.
Harker, David E.
Kelley, Michael S.
Woodward, Charles E.
Murphy, Jim R.
TI ABSORPTION EFFICIENCIES OF FORSTERITE. I. DISCRETE DIPOLE APPROXIMATION
EXPLORATIONS IN GRAIN SHAPE AND SIZE
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE circumstellar matter; comets: general; infrared: planetary systems;
line: profiles; methods: numerical; protoplanetary disks
ID PROTOPLANETARY ACCRETION DISKS; COMET HALE-BOPP; SILICATE DUST; COSMIC
DUST; OPTICAL-PROPERTIES; INFRARED-SPECTRA; 3-DIMENSIONAL STRUCTURES;
NONSPHERICAL PARTICLES; CRYSTALLINE SILICATE; INTERPLANETARY DUST
AB We compute the absorption efficiency (Q(abs)) of forsterite using the discrete dipole approximation in order to identify and describe what characteristics of crystal grain shape and size are important to the shape, peak location, and relative strength of spectral features in the 8-40 mu m wavelength range. Using the DDSCAT code, we compute Q(abs) for non-spherical polyhedral grain shapes with a(eff) =0.1 mu m. The shape characteristics identified are (1) elongation/reduction along one of three crystallographic axes; (2) asymmetry, such that all three crystallographic axes are of different lengths; and (3) the presence of crystalline faces that are not parallel to a specific crystallographic axis, e.g., non-rectangular prisms and (di) pyramids. Elongation/reduction dominates the locations and shapes of spectral features near 10, 11, 16, 23.5, 27, and 33.5 mu m, while asymmetry and tips are secondary shape effects. Increasing grain sizes (0.1-1.0 mu m) shifts the 10 and 11 mu m features systematically toward longer wavelengths and relative to the 11 mu m feature increases the strengths and slightly broadens the longer wavelength features. Seven spectral shape classes are established for crystallographic a-, b-, and c-axes and include columnar and platelet shapes plus non-elongated or equant grain shapes. The spectral shape classes and the effects of grain size have practical application in identifying or excluding columnar, platelet, or equant forsterite grain shapes in astrophysical environs. Identification of the shape characteristics of forsterite from 8 to 40 mu m spectra provides a potential means to probe the temperatures at which forsterite formed.
C1 [Lindsay, Sean S.] Univ Tennessee, Dept Earth & Planetary Sci, Knoxville, TN 37996 USA.
[Wooden, Diane H.] NASA, Div Space Sci, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Harker, David E.] Univ Calif San Diego, Ctr Astrophys & Space Sci, La Jolla, CA 92093 USA.
[Kelley, Michael S.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Woodward, Charles E.] Univ Minnesota, Minnesota Inst Astrophys, Minneapolis, MN 55455 USA.
[Murphy, Jim R.] New Mexico State Univ, Dept Astron, Las Cruces, NM 88003 USA.
RP Lindsay, SS (reprint author), Univ Tennessee, Dept Earth & Planetary Sci, 1421 Circle Dr, Knoxville, TN 37996 USA.
EM slindsay@utk.edu; diane.h.wooden@nasa.gov; dharker@uscd.edu;
msk@astro.umd.edu; chelsea@astro.umn.edu; murphy@nmsu.edu
OI Harker, David/0000-0001-6397-9082; Kelley, Michael/0000-0002-6702-7676
FU Planetary Systems Branch of the NASA Ames Research Center
[NNX08AV43H/114]; Planetary Atmospheres Program [08-PATM08-0080]; NAS
[SMD-09-1144, SMD-10-1637, SMD-11-2361]
FX We express special appreciation for laboratory experimentalists Dr.
Akemi Tamanai and Dr. Chioye Koike for sharing electronic versions of
data published by the Jena and Kyoto groups, respectively. We thank
summer intern Brittany M. Hunter (University of Western Australia) for
working with D.H.W. on in-depth analyses of asymmetric bricks. The
authors wish to thank the efforts of an anonymous referee, whose
suggestions and critique greatly improved the manuscript. S.S.L. thanks
the Planetary Systems Branch of the NASA Ames Research Center for
hosting him as a GSRP Fellow (grant No. NNX08AV43H/114) during his three
12 week GSRP Summer visits. He also expresses his strongest gratitude to
D.H.W. for all the long hours and hard work she contributed to this
paper. Her efforts are greatly appreciated! S.S.L. also thanks J.R.M.
for his guidance in assembling this paper. D.H.W., D.E.H., and M.S.K.
acknowledge significant support from the Planetary Atmospheres
(08-PATM08-0080) Program. The DDSCAT computations utilized NAS time
allocations (SMD-09-1144, SMD-10-1637, and SMD-11-2361) awarded to
D.H.W. by competitive process for the associated approved PATM research
program. S.S.L. thanks C.E.W. for insightful edits and masterful
wordsmithing. S.S.L. and D.H.W. also thank Zack Gainsforth for his
insights into the unit cell structure and crystal habit of forsterite.
We thank J. Bradley, H. Mutschke, Th. Henning, and C. Jager for comments
during the progress of the analyses.
NR 85
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PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD MAR 20
PY 2013
VL 766
IS 1
AR 54
DI 10.1088/0004-637X/766/1/54
PG 25
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 105GH
UT WOS:000316054000054
ER
PT J
AU Sakamoto, T
Troja, E
Aoki, K
Guiriec, S
Im, M
Leloudas, G
Malesani, D
Melandri, A
Postigo, AD
Urata, Y
Xu, D
D'Avanzo, P
Gorosabel, J
Jeon, Y
Sanchez-Ramirez, R
Andersen, MI
Bai, J
Barthelmy, SD
Briggs, MS
Foley, S
Fruchter, AS
Fynbo, JPU
Gehrels, N
Huang, K
Jang, M
Kawai, N
Korhonen, H
Mao, J
Norris, JP
Preece, RD
Racusin, JL
Thoene, CC
Vida, K
Zhao, X
AF Sakamoto, T.
Troja, E.
Aoki, K.
Guiriec, S.
Im, M.
Leloudas, G.
Malesani, D.
Melandri, A.
de Ugarte Postigo, A.
Urata, Y.
Xu, D.
D'Avanzo, P.
Gorosabel, J.
Jeon, Y.
Sanchez-Ramirez, R.
Andersen, M. I.
Bai, J.
Barthelmy, S. D.
Briggs, M. S.
Foley, S.
Fruchter, A. S.
Fynbo, J. P. U.
Gehrels, N.
Huang, K.
Jang, M.
Kawai, N.
Korhonen, H.
Mao, J.
Norris, J. P.
Preece, R. D.
Racusin, J. L.
Thoene, C. C.
Vida, K.
Zhao, X.
TI IDENTIFYING THE LOCATION IN THE HOST GALAXY OF THE SHORT GRB 111117A
WITH THE CHANDRA SUBARCSECOND POSITION
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE gamma-ray burst: individual (GRB 111117A)
ID GAMMA-RAY BURSTS; STAR-FORMATION RATES; NEUTRON-STAR; OPTICAL
AFTERGLOWS; COMPLETE SAMPLE; HIGH-REDSHIFT; LIGHT CURVES; EMISSION;
PROGENITORS; TELESCOPE
AB We present our successful Chandra program designed to identify, with subarcsecond accuracy, the X-ray afterglow of the short GRB 111117A, which was discovered by Swift and Fermi. Thanks to our rapid target of opportunity request, Chandra clearly detected the X-ray afterglow, though no optical afterglow was found in deep optical observations. The host galaxy was clearly detected in the optical and near-infrared band, with the best photometric redshift of z = 1.31(-0.23)(+0.46) (90% confidence), making it one of the highest known short gamma-ray burst ( GRB) redshifts. Furthermore, we see an offset of 1.0 +/- 0.2 arcsec, which corresponds to 8.4 +/- 1.7 kpc, between the host and the afterglow position. We discuss the importance of using Chandra for obtaining subarcsecond X-ray localizations of short GRB afterglows to study GRB environments.
C1 [Sakamoto, T.; Troja, E.] NASA, Goddard Space Flight Ctr, CRESST, Greenbelt, MD 20771 USA.
[Sakamoto, T.] Univ Maryland Baltimore Cty, Joint Ctr Astrophys, Baltimore, MD 21250 USA.
[Sakamoto, T.; Troja, E.; Guiriec, S.; Barthelmy, S. D.; Gehrels, N.; Racusin, J. L.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Sakamoto, T.] Aoyama Gakuin Univ, Dept Math & Phys, Coll Sci & Engn, Chuo Ku, Sagamihara, Kanagawa 2525258, Japan.
[Troja, E.] Univ Maryland, Dept Astron, Joint Ctr Astrophys, College Pk, MD 20742 USA.
[Aoki, K.] Natl Inst Nat Sci, Natl Astron Observ Japan, Subaru Telescope, Hilo, HI 96720 USA.
[Im, M.; Jeon, Y.; Jang, M.] Seoul Natl Univ, Dept Phys & Astron, CEOU, Seoul 151747, South Korea.
[Leloudas, G.; Malesani, D.; de Ugarte Postigo, A.; Andersen, M. I.; Fynbo, J. P. U.] Univ Copenhagen, Niels Bohr Inst, Dark Cosmol Ctr, DK-2100 Copenhagen O, Denmark.
[Leloudas, G.] Stockholm Univ, Dept Phys, Oskar Klein Ctr, SE-10691 Stockholm, Sweden.
[Melandri, A.; D'Avanzo, P.] INAF Osservatorio Astron Brera, I-23807 Merate, LC, Italy.
[de Ugarte Postigo, A.; Gorosabel, J.; Sanchez-Ramirez, R.; Thoene, C. C.] CSIC, Inst Astrofis Andalucia, E-18008 Granada, Spain.
[Urata, Y.] Natl Cent Univ, Inst Astron, Chungli 32054, Taiwan.
[Xu, D.] Weizmann Inst Sci, Dept Particle Phys & Astron, IL-76100 Rehovot, Israel.
[Andersen, M. I.; Korhonen, H.] Univ Copenhagen, Niels Bohr Inst, DK-2100 Copenhagen, Denmark.
[Bai, J.; Mao, J.; Zhao, X.] Chinese Acad Sci, Yunnan Astron Observ, Kunming 650011, Yunnan Province, Peoples R China.
[Bai, J.; Mao, J.; Zhao, X.] Chinese Acad Sci, Key Lab Struct & Evolut Celestial Objects, Kunming 650011, Peoples R China.
[Briggs, M. S.; Preece, R. D.] Univ Alabama, Ctr Space Plasma & Aeron Res, Huntsville, AL 35805 USA.
[Foley, S.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany.
[Fruchter, A. S.] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
[Huang, K.] Acad Sinica, Inst Astron & Astrophys, Taipei 106, Taiwan.
[Kawai, N.] Tokyo Inst Technol, Dept Phys, Meguro Ku, Tokyo 1528551, Japan.
[Korhonen, H.] Univ Copenhagen, Nat Hist Museum Denmark, Ctr Star & Planet Format, DK-1350 Copenhagen, Denmark.
[Mao, J.] Korea Astron & Space Sci Inst, Div Space Sci, Taejon 305348, South Korea.
[Norris, J. P.] Boise State Univ, Dept Phys, Boise, ID 83725 USA.
[Vida, K.] Hungarian Acad Sci, Konkoly Observ, H-1121 Budapest XII, Hungary.
RP Sakamoto, T (reprint author), NASA, Goddard Space Flight Ctr, CRESST, Greenbelt, MD 20771 USA.
RI Fynbo, Johan/L-8496-2014; Korhonen, Heidi/E-3065-2016;
OI Fynbo, Johan/0000-0002-8149-8298; Korhonen, Heidi/0000-0003-0529-1161;
Preece, Robert/0000-0003-1626-7335; Thone,
Christina/0000-0002-7978-7648; Im, Myungshin/0000-0002-8537-6714; de
Ugarte Postigo, Antonio/0000-0001-7717-5085; Sanchez-Ramirez,
Ruben/0000-0002-7158-5099
FU Swift mission [NNX12AE75G]; Danish National Research Foundation; Chandra
Cycle 13 grant [GO2-13084X]; Spanish research projects [AYA2011-24780/
ESP, AYA200914000-C03-01/ESP, AYA2010-21887-C04-01]; Swedish Research
Council [623-2011-7117]; Hungarian Science Research Program (OTKA)
[K-81421]; "Lendulet" Young Researchers' Program of the Hungarian
Academy of Sciences; European Commission under the Marie Curie IEF
Programme; Creative Research Initiative program, of the National
Research Foundation of Korea (NRFK) [2010-0000712]; Korean government
(MEST)
FX We would like to thank the anonymous referee for comments and
suggestions that materially improved the paper. This work made use of
data supplied by the UK Swift Science Data Centre at theUniversity of
Leicester. This work is based on observations using the United Kingdom
Infrared Telescope, which is operated by the Joint Astronomy Centre on
behalf of the Science and Technology Facilities Council of the U.K. with
a partial support by Swift mission (e.g., Swift Cycle 7 GI grant
NNX12AE75G) and the Gran Telescopio Canarias (GTC), installed in the
Spanish Observatorio del Roque de los Muchachos of the Instituto de
Astrofisica de Canarias, on the island of La Palma. The Dark Cosmology
Centre is funded by the Danish National Research Foundation. This
research is partly based on observations made with the Nordic Optical
Telescope, operated on the island of La Palma jointly by Denmark,
Finland, Iceland, Norway, and Sweden, in the Spanish Observatorio del
Roque de los Muchachos of the Instituto de Astrofisica de Canarias. This
work was supported by Chandra Cycle 13 grant GO2-13084X. The research
activity of A.d.U.P., C.C.T., R.S.R., and J.G. is supported by Spanish
research projects AYA2011-24780/ ESP, AYA200914000-C03-01/ESP and
AYA2010-21887-C04-01. G. L. is supported by the Swedish Research Council
through grant No. 623-2011-7117. K.V. is grateful to the Hungarian
Science Research Program (OTKA) for support under the grant K-81421.
This work is supported by the "Lendulet" Young Researchers' Program of
the Hungarian Academy of Sciences. H.K. acknowledges the support from
the European Commission under the Marie Curie IEF Programme in FP7. M.I.
and Y.J. were supported by the Creative Research Initiative program, No.
2010-0000712, of the National Research Foundation of Korea (NRFK) funded
by the Korean government (MEST).
NR 81
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U2 12
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD MAR 20
PY 2013
VL 766
IS 1
AR 41
DI 10.1088/0004-637X/766/1/41
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 105GH
UT WOS:000316054000041
ER
PT J
AU Seifina, E
Titarchuk, L
Frontera, F
AF Seifina, Elena
Titarchuk, Lev
Frontera, Filippo
TI STABILITY OF THE PHOTON INDICES IN Z-SOURCE GX 340+0 FOR SPECTRAL STATES
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE accretion, accretion disks; black hole physics; radiation mechanisms:
non-thermal; stars: individual (GX 340+0); stars: neutron
ID QUASI-PERIODIC OSCILLATIONS; X-RAY BINARIES; Z-SOURCE GX-340+0; CYGNUS
X-2; NEUTRON-STAR; Z-TRACK; ASTRONOMY SATELLITE; TIMING BEHAVIOR; XTE
J1701-462; 4U 1728-34
AB We show an analysis of the spectral and timing properties of X-ray radiation from Z-source GX 340+0 during its evolution when the electron temperature of the transition layer (TL) kT(e) monotonically decreases from 21 to 3 keV. We analyze episodes observed with BeppoSAX and RXTE. We reveal that the X-ray broadband energy spectra during all spectral states can be reproduced by a physical model composed of a soft Blackbody component and two Comptonized components (both due to the presence of the TL that upscatters both seed photons of T-s1 less than or similar to 1 keV coming from the disk (first component Comptb1), and seed photons of temperature T-s2 less than or similar to 1.5 keV coming from the neutron star (second component Comptb2) and the iron-line (Gaussian) component. Spectral analysis using this model indicates that the photon power-law indices Gamma(com1) and Gamma(com2) of the Comptonized components are almost constant, Gamma(com1) and Gamma(com2) similar to 2 when kT(e) changes from 3 to 21 keV along the Z-track. We interpret the detected quasi-stability of the indices of Comptonized components to be near a value of 2. Furthermore, this index stability now found for the Comptonized spectral components of Z-source GX 340+0 is similar to that previously established in the atoll sources 4U 1728-34 and GX 3+1, and earlier proposed for a number of X-ray neutron stars (NSs). This behavior of NSs both for atoll and Z-sources is essentially different from that observed in black hole binaries where Gamma(com) increases during a spectral evolution from the low state to the high state and ultimately saturates at a high mass accretion rate.
C1 [Seifina, Elena] Moscow MV Lomonosov State Univ, Sternberg Astron Inst, Moscow 119992, Russia.
[Titarchuk, Lev; Frontera, Filippo] Univ Ferrara, Dipartimento Fis, I-44122 Ferrara, Italy.
[Titarchuk, Lev] George Mason Univ, Coll Sci, Fairfax, VA 22030 USA.
[Titarchuk, Lev] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20770 USA.
RP Seifina, E (reprint author), Moscow MV Lomonosov State Univ, Sternberg Astron Inst, Univ Prospect 13, Moscow 119992, Russia.
EM seif@sai.msu.ru; titarchuk@fe.infn.it; frontera@fe.infn.it
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
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JI Astrophys. J.
PD MAR 20
PY 2013
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DI 10.1088/0004-637X/766/1/63
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SC Astronomy & Astrophysics
GA 105GH
UT WOS:000316054000063
ER
PT J
AU Shannon, RM
Cordes, JM
Metcalfe, TS
Lazio, TJW
Cognard, I
Desvignes, G
Janssen, GH
Jessner, A
Kramer, M
Lazaridis, K
Purver, MB
Stappers, BW
Theureau, G
AF Shannon, R. M.
Cordes, J. M.
Metcalfe, T. S.
Lazio, T. J. W.
Cognard, I.
Desvignes, G.
Janssen, G. H.
Jessner, A.
Kramer, M.
Lazaridis, K.
Purver, M. B.
Stappers, B. W.
Theureau, G.
TI AN ASTEROID BELT INTERPRETATION FOR THE TIMING VARIATIONS OF THE
MILLISECOND PULSAR B1937+21
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE minor planets, asteroids: general; pulsars: general; pulsars: individual
(PSR B1937+21); stars: neutron
ID NEUTRON-STAR; PLANETARY SYSTEM; BINARY-SYSTEMS; GRAVITATIONAL-WAVES;
SOLAR-SYSTEM; WHITE-DWARFS; PSR B1913+16; SPIN-DOWN; PRECISION; DEBRIS
AB Pulsar timing observations have revealed companions to neutron stars that include other neutron stars, white dwarfs, main-sequence stars, and planets. We demonstrate that the correlated and apparently stochastic residual times of arrival from the millisecond pulsar B1937+21 are consistent with the signature of an asteroid belt having a total mass less than or similar to 0.05M (R). Unlike the solar system's asteroid belt, the best fit pulsar asteroid belt extends over a wide range of radii, consistent with the absence of any shepherding companions. We suggest that any pulsar that has undergone accretion-driven spin-up and subsequently evaporated its companion may harbor orbiting asteroid mass objects. The resulting timing variations may fundamentally limit the timing precision of some of the other millisecond pulsars. Observational tests of the asteroid belt model include identifying periodicities from individual asteroids, which are difficult; testing for statistical stationarity, which becomes possible when observations are conducted over a longer observing span; and searching for reflected radio emission.
C1 [Shannon, R. M.; Cordes, J. M.] Cornell Univ, Dept Astron, Ithaca, NY 14853 USA.
[Metcalfe, T. S.] Space Sci Inst, Boulder, CO 80301 USA.
[Lazio, T. J. W.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Cognard, I.; Desvignes, G.; Theureau, G.] Univ Orleans, CNRS, LPC2E, F-45071 Orleans 2, France.
[Cognard, I.; Desvignes, G.; Theureau, G.] Observ Paris, Stn Radioastron Nancay, Paris, France.
[Desvignes, G.; Jessner, A.; Kramer, M.; Lazaridis, K.] Max Planck Inst Radioastron, D-53121 Bonn, Germany.
[Janssen, G. H.; Kramer, M.; Purver, M. B.; Stappers, B. W.] Univ Manchester, Manchester M13 9PL, Lancs, England.
[Janssen, G. H.; Kramer, M.; Purver, M. B.; Stappers, B. W.] Jodrell Bank Observ, Manchester M13 9PL, Lancs, England.
RP Shannon, RM (reprint author), Cornell Univ, Dept Astron, Ithaca, NY 14853 USA.
EM ryan.shannon@csiro.au; cordes@astro.cornell.edu
OI Shannon, Ryan/0000-0002-7285-6348; Metcalfe, Travis/0000-0003-4034-0416
FU NSF [AST-0807151]; Research Experience for Undergraduates Program; NAIC;
Netherlands Foundation for Scientific Research (NWO); National
Aeronautics and Space Administration
FX We thank the referee for comments that improved the quality of this
paper. This work was supported by the NSF through grant AST-0807151 and
the Research Experience for Undergraduates Program. This work was also
supported by NAIC, when it was operated by Cornell University under a
cooperative agreement with the NSF. Part of this research was carried
out at the Jet Propulsion Laboratory, California Institute of
Technology, under a contract with the National Aeronautics and Space
Administration. This work is partially based on observations with the
100 m telescope of the Max-Planck-Institut fur Radioastronomie (MPIfR)
at Effelsberg, Germany. The Westerbork Synthesis Radio Telescope is
operated by ASTRON(Netherlands Foundation for Research in Astronomy)
with support from the Netherlands Foundation for Scientific Research
(NWO). The Nancay Radio Observatory is operated by the Paris
Observatory, associated to the French Centre National de la Recherche
Scientifique (CNRS). The Nancay Observatory also gratefully acknowledges
the financial support of the Region Centre in France. This work made use
of NASA's ADS System.
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD MAR 20
PY 2013
VL 766
IS 1
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DI 10.1088/0004-637X/766/1/5
PG 14
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 105GH
UT WOS:000316054000005
ER
PT J
AU Tremmel, M
Fragos, T
Lehmer, BD
Tzanavaris, P
Belczynski, K
Kalogera, V
Basu-Zych, AR
Farr, WM
Hornschemeier, A
Jenkins, L
Ptak, A
Zezas, A
AF Tremmel, M.
Fragos, T.
Lehmer, B. D.
Tzanavaris, P.
Belczynski, K.
Kalogera, V.
Basu-Zych, A. R.
Farr, W. M.
Hornschemeier, A.
Jenkins, L.
Ptak, A.
Zezas, A.
TI MODELING THE REDSHIFT EVOLUTION OF THE NORMAL GALAXY X-RAY LUMINOSITY
FUNCTION
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE binaries: close; galaxies: stellar content; stars: evolution; X-rays:
binaries; X-rays: diffuse background; X-rays: galaxies
ID DEEP FIELD-SOUTH; STAR-FORMATION HISTORY; BLACK-HOLE BINARIES; ACTIVE
GALACTIC NUCLEI; INITIAL MASS FUNCTIONS; SIMILAR-TO 1; FORMING GALAXIES;
STELLAR-MASS; HOT GAS; EXPLOSION MECHANISM
AB Emission from X-ray binaries (XRBs) is a major component of the total X-ray luminosity of normal galaxies, so X-ray studies of high-redshift galaxies allow us to probe the formation and evolution of XRBs on very long timescales (similar to 10 Gyr). In this paper, we present results from large-scale population synthesis models of binary populations in galaxies from z = 0 to similar to 20. We use as input into our modeling the Millennium II Cosmological Simulation and the updated semi-analytic galaxy catalog by Guo et al. to self-consistently account for the star formation history (SFH) and metallicity evolution of each galaxy. We run a grid of 192 models, varying all the parameters known from previous studies to affect the evolution of XRBs. We use our models and observationally derived prescriptions for hot gas emission to create theoretical galaxy X-ray luminosity functions (XLFs) for several redshift bins. Models with low common envelope efficiencies, a 50% twins mass ratio distribution, a steeper initial mass function exponent, and high stellar wind mass-loss rates best match observational results from Tzanavaris & Georgantopoulos, though they significantly underproduce bright early-type and very bright (L-x > 10(41)) late-type galaxies. These discrepancies are likely caused by uncertainties in hot gas emission and SFHs, active galactic nucleus contamination, and a lack of dynamically formed low-mass XRBs. In our highest likelihood models, we find that hot gas emission dominates the emission for most bright galaxies. We also find that the evolution of the normal galaxy X-ray luminosity density out to z = 4 is driven largely by XRBs in galaxies with X-ray luminosities between 10(40) and 10(41) erg s(-1).
C1 [Tremmel, M.] Univ Washington, Dept Astron, Seattle, WA 98195 USA.
[Fragos, T.; Zezas, A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Lehmer, B. D.; Tzanavaris, P.] Johns Hopkins Univ, Baltimore, MD 21218 USA.
[Lehmer, B. D.; Tzanavaris, P.; Basu-Zych, A. R.; Hornschemeier, A.; Jenkins, L.; Ptak, A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Belczynski, K.] Univ Warsaw, Astron Observ, PL-00478 Warsaw, Poland.
[Belczynski, K.] Univ Texas Brownsville, Ctr Gravitat Wave Astron, Brownsville, TX 78520 USA.
[Kalogera, V.; Farr, W. M.] Northwestern Univ, Ctr Interdisciplinary Res & Explorat Astrophys, Evanston, IL 60208 USA.
[Kalogera, V.; Farr, W. M.] Northwestern Univ, Dept Phys & Astron, Evanston, IL 60208 USA.
[Zezas, A.] Univ Crete, Dept Phys, Iraklion 71003, Crete, Greece.
[Zezas, A.] Fdn Res & Technol, IESL, Iraklion 71110, Crete, Greece.
RP Tremmel, M (reprint author), Univ Washington, Dept Astron, Box 351580, Seattle, WA 98195 USA.
EM mjt29@astro.washington.edu
RI Zezas, Andreas/C-7543-2011; Fragos, Tassos/A-3581-2016
OI Zezas, Andreas/0000-0001-8952-676X; Fragos, Tassos/0000-0003-1474-1523
FU CfA; ITC; NASA at Goddard Space Flight Center; MSHE [N203 404939]; NASA
ADP [NNX12AL39G]
FX The authors thank the anonymous referee whose comments and suggestions
have helped to improve this paper. T.F. acknowledges support from the
CfA and the ITC prize fellowship programs. B.D.L. thanks the Einstein
Fellowship program. P.T. acknowledges support through a NASA
Post-doctoral Program Fellowship at Goddard Space Flight Center,
administered by Oak Ridge Associated Universities through a contract
with NASA. Resources supporting this work were provided by the
Northwestern University Quest High Performance Computing (HPC) cluster
and by the NASA High-End Computing (HEC) Program through the NASA Center
for Climate Simulation (NCCS) at Goddard Space Flight Center. K.B.
acknowledges support from MSHE grant N203 404939. V.K. acknowledges
support for this work from NASA ADP grant NNX12AL39G (sub-contract to
Northwestern University)
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD MAR 20
PY 2013
VL 766
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AR 19
DI 10.1088/0004-637X/766/1/19
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 105GH
UT WOS:000316054000019
ER
PT J
AU Waldmann, IP
Tinetti, G
Deroo, P
Hollis, MDJ
Yurchenko, SN
Tennyson, J
AF Waldmann, I. P.
Tinetti, G.
Deroo, P.
Hollis, M. D. J.
Yurchenko, S. N.
Tennyson, J.
TI BLIND EXTRACTION OF AN EXOPLANETARY SPECTRUM THROUGH INDEPENDENT
COMPONENT ANALYSIS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE methods: data analysis; methods: observational; methods: statistical;
planets and satellites: atmospheres; planets and satellites: individual
(HD189733b); techniques: spectroscopic
ID HUBBLE-SPACE-TELESCOPE; TRANSITING HOT JUPITER; METAL-RICH ATMOSPHERE;
SUPER-EARTH GJ1214B; PLANET HD 209458B; EXTRASOLAR PLANET; TRANSMISSION
SPECTROSCOPY; LIGHT CURVES; EMISSION-SPECTRUM; DAYSIDE SPECTRUM
AB Blind-source separation techniques are used to extract the transmission spectrum of the hot-Jupiter HD189733b recorded by the Hubble/NICMOS instrument. Such a "blind" analysis of the data is based on the concept of independent component analysis. The detrending of Hubble/NICMOS data using the sole assumption that nongaussian systematic noise is statistically independent from the desired light-curve signals is presented. By not assuming any prior or auxiliary information but the data themselves, it is shown that spectroscopic errors only about 10%-30% larger than parametric methods can be obtained for 11 spectral bins with bin sizes of similar to 0.09 mu m. This represents a reasonable trade-off between a higher degree of objectivity for the non-parametric methods and smaller standard errors for the parametric de-trending. Results are discussed in light of previous analyses published in the literature. The fact that three very different analysis techniques yield comparable spectra is a strong indication of the stability of these results.
C1 [Waldmann, I. P.; Tinetti, G.; Hollis, M. D. J.; Yurchenko, S. N.; Tennyson, J.] UCL, Dept Phys & Astron, London WC1E 6BT, England.
[Deroo, P.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Waldmann, IP (reprint author), UCL, Dept Phys & Astron, Gower St, London WC1E 6BT, England.
EM ingo@star.ucl.ac.uk
RI Tennyson, Jonathan/I-2222-2012; Yurchenko, Sergey/G-9929-2012;
OI Tennyson, Jonathan/0000-0002-4994-5238; Yurchenko,
Sergey/0000-0001-9286-9501; Hollis, Morgan/0000-0002-8058-9075; Tinetti,
Giovanna/0000-0001-6058-6654
FU ERC [267219]; STFC; NERC; UKSA; UCL; Royal Society; NASA [NAS5-26555];
NASA Office of Space Science [NNX09AF08G]
FX The authors thank Mark Swain and Filipe Abdalla for helpful discussions.
This work is supported by ERC Advanced Investigator Project 267219,
STFC, NERC, UKSA, UCL and the Royal Society. All of the data presented
in this paper were obtained from the Multimission Archive at the Space
Telescope Science Institute (MAST). STScI is operated by the Association
of Universities for Research in Astronomy, Inc., under NASA contract
NAS5-26555. Support for MAST for non-HST data is provided by the NASA
Office of Space Science via grant NNX09AF08G and by other grants and
contracts.
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SN 0004-637X
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JI Astrophys. J.
PD MAR 20
PY 2013
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DI 10.1088/0004-637X/766/1/7
PG 9
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 105GH
UT WOS:000316054000007
ER
PT J
AU Aartsen, MG
Abbasi, R
Abdou, Y
Ackermann, M
Adams, J
Aguilar, JA
Ahlers, M
Altmann, D
Andeen, K
Auffenberg, J
Bai, X
Baker, M
Barwick, SW
Baum, V
Bay, R
Beattie, K
Beatty, JJ
Bechet, S
Tjus, JB
Becker, KH
Bell, M
Benabderrahmane, ML
BenZvi, S
Berdermann, J
Berghaus, P
Berley, D
Bernardini, E
Bertrand, D
Besson, DZ
Bindig, D
Bissok, M
Blaufuss, E
Blumenthal, J
Boersma, DJ
Bohaichuk, S
Bohm, C
Bose, D
Boser, S
Botner, O
Brayeur, L
Brown, AM
Bruijn, R
Brunner, J
Buitink, S
Carson, M
Casey, J
Casier, M
Chirkin, D
Christy, B
Clark, K
Clevermann, F
Cohen, S
Cowen, DF
Silva, AHC
Danninger, M
Daughhetee, J
Davis, JC
De Clercq, C
De Ridder, S
Descamps, F
Desiati, P
de Vries-Uiterweerd, G
DeYoung, T
Diaz-Velez, JC
Dreyer, J
Dumm, JP
Dunkman, M
Eagan, R
Eisch, J
Ellsworth, RW
Engdegard, O
Euler, S
Evenson, PA
Fadiran, O
Fazely, AR
Fedynitch, A
Feintzeig, J
Feusels, T
Filimonov, K
Finley, C
Fischer-Wasels, T
Flis, S
Franckowiak, A
Franke, R
Frantzen, K
Fuchs, T
Gaisser, TK
Gallagher, J
Gerhardt, L
Gladstone, L
Glusenkamp, T
Goldschmidt, A
Golup, G
Goodman, JA
Gora, D
Grant, D
Gross, A
Grullon, S
Gurtner, M
Ha, C
Ismail, AH
Hallgren, A
Halzen, F
Hanson, K
Heereman, D
Heimann, P
Heinen, D
Helbing, K
Hellauer, R
Hickford, S
Hill, GC
Hoffman, KD
Hoffmann, R
Homeier, A
Hoshina, K
Huelsnitz, W
Hulth, PO
Hultqvist, K
Hussain, S
Ishihara, A
Jacobi, E
Jacobsen, J
Japaridze, GS
Jlelati, O
Kappes, A
Karg, T
Karle, A
Kiryluk, J
Kislat, F
Klas, J
Klein, SR
Kohne, JH
Kohnen, G
Kolanoski, H
Kopke, L
Kopper, C
Kopper, S
Koskinen, DJ
Kowalski, M
Krasberg, M
Kroll, G
Kunnen, J
Kurahashi, N
Kuwabara, T
Labare, M
Landsman, H
Larson, MJ
Lauer, R
Lesiak-Bzdak, M
Lunemann, J
Madsen, J
Maruyama, R
Mase, K
Matis, HS
McNally, F
Meagher, K
Merck, M
Meszaros, P
Meures, T
Miarecki, S
Middell, E
Milke, N
Miller, J
Mohrmann, L
Montaruli, T
Morse, R
Nahnhauer, R
Naumann, U
Nowicki, SC
Nygren, DR
Obertacke, A
Odrowski, S
Olivas, A
Olivo, M
O'Murchadha, A
Panknin, S
Paul, L
Pepper, JA
de los Heros, CP
Pieloth, D
Pirk, N
Posselt, J
Price, PB
Przybylski, GT
Radel, L
Rawlins, K
Redl, P
Resconi, E
Rhode, W
Ribordy, M
Richman, M
Riedel, B
Rodrigues, JP
Rothmaier, F
Rott, C
Ruhe, T
Ruzybayev, B
Ryckbosch, D
Saba, SM
Salameh, T
Sander, HG
Santander, M
Sarkar, S
Schatto, K
Scheel, M
Scheriau, F
Schmidt, T
Schmitz, M
Schoenen, S
Schoneberg, S
Schonherr, L
Schonwald, A
Schukraft, A
Schulte, L
Schulz, O
Seckel, D
Seo, SH
Sestayo, Y
Seunarine, S
Sheremata, C
Smith, MWE
Soiron, M
Soldin, D
Spiczak, GM
Spiering, C
Stamatikos, M
Stanev, T
Stasik, A
Stezelberger, T
Stokstad, RG
Stossl, A
Strahler, EA
Strom, R
Sullivan, GW
Taavola, H
Taboada, I
Tamburro, A
Ter-Antonyan, S
Tilav, S
Toale, PA
Toscano, S
Usner, M
van der Drift, D
van Eijndhoven, N
Van Overloop, A
van Santen, J
Vehring, M
Voge, M
Vraeghe, M
Walck, C
Waldenmaier, T
Wallraff, M
Walter, M
Wasserman, R
Weaver, C
Wendt, C
Westerhoff, S
Whitehorn, N
Wiebe, K
Wiebusch, CH
Williams, DR
Wissing, H
Wolf, M
Wood, TR
Woschnagg, K
Xu, C
Xu, DL
Xu, XW
Yanez, JP
Yodh, G
Yoshida, S
Zarzhitsky, P
Ziemann, J
Zierke, S
Zilles, A
Zoll, M
AF Aartsen, M. G.
Abbasi, R.
Abdou, Y.
Ackermann, M.
Adams, J.
Aguilar, J. A.
Ahlers, M.
Altmann, D.
Andeen, K.
Auffenberg, J.
Bai, X.
Baker, M.
Barwick, S. W.
Baum, V.
Bay, R.
Beattie, K.
Beatty, J. J.
Bechet, S.
Tjus, J. Becker
Becker, K. -H.
Bell, M.
Benabderrahmane, M. L.
BenZvi, S.
Berdermann, J.
Berghaus, P.
Berley, D.
Bernardini, E.
Bertrand, D.
Besson, D. Z.
Bindig, D.
Bissok, M.
Blaufuss, E.
Blumenthal, J.
Boersma, D. J.
Bohaichuk, S.
Bohm, C.
Bose, D.
Boeser, S.
Botner, O.
Brayeur, L.
Brown, A. M.
Bruijn, R.
Brunner, J.
Buitink, S.
Carson, M.
Casey, J.
Casier, M.
Chirkin, D.
Christy, B.
Clark, K.
Clevermann, F.
Cohen, S.
Cowen, D. F.
Silva, A. H. Cruz
Danninger, M.
Daughhetee, J.
Davis, J. C.
De Clercq, C.
De Ridder, S.
Descamps, F.
Desiati, P.
de Vries-Uiterweerd, G.
DeYoung, T.
Diaz-Velez, J. C.
Dreyer, J.
Dumm, J. P.
Dunkman, M.
Eagan, R.
Eisch, J.
Ellsworth, R. W.
Engdegard, O.
Euler, S.
Evenson, P. A.
Fadiran, O.
Fazely, A. R.
Fedynitch, A.
Feintzeig, J.
Feusels, T.
Filimonov, K.
Finley, C.
Fischer-Wasels, T.
Flis, S.
Franckowiak, A.
Franke, R.
Frantzen, K.
Fuchs, T.
Gaisser, T. K.
Gallagher, J.
Gerhardt, L.
Gladstone, L.
Gluesenkamp, T.
Goldschmidt, A.
Golup, G.
Goodman, J. A.
Gora, D.
Grant, D.
Gross, A.
Grullon, S.
Gurtner, M.
Ha, C.
Ismail, A. Haj
Hallgren, A.
Halzen, F.
Hanson, K.
Heereman, D.
Heimann, P.
Heinen, D.
Helbing, K.
Hellauer, R.
Hickford, S.
Hill, G. C.
Hoffman, K. D.
Hoffmann, R.
Homeier, A.
Hoshina, K.
Huelsnitz, W.
Hulth, P. O.
Hultqvist, K.
Hussain, S.
Ishihara, A.
Jacobi, E.
Jacobsen, J.
Japaridze, G. S.
Jlelati, O.
Kappes, A.
Karg, T.
Karle, A.
Kiryluk, J.
Kislat, F.
Klaes, J.
Klein, S. R.
Koehne, J-H.
Kohnen, G.
Kolanoski, H.
Koepke, L.
Kopper, C.
Kopper, S.
Koskinen, D. J.
Kowalski, M.
Krasberg, M.
Kroll, G.
Kunnen, J.
Kurahashi, N.
Kuwabara, T.
Labare, M.
Landsman, H.
Larson, M. J.
Lauer, R.
Lesiak-Bzdak, M.
Luenemann, J.
Madsen, J.
Maruyama, R.
Mase, K.
Matis, H. S.
McNally, F.
Meagher, K.
Merck, M.
Meszaros, P.
Meures, T.
Miarecki, S.
Middell, E.
Milke, N.
Miller, J.
Mohrmann, L.
Montaruli, T.
Morse, R.
Nahnhauer, R.
Naumann, U.
Nowicki, S. C.
Nygren, D. R.
Obertacke, A.
Odrowski, S.
Olivas, A.
Olivo, M.
O'Murchadha, A.
Panknin, S.
Paul, L.
Pepper, J. A.
de los Heros, C. Perez
Pieloth, D.
Pirk, N.
Posselt, J.
Price, P. B.
Przybylski, G. T.
Raedel, L.
Rawlins, K.
Redl, P.
Resconi, E.
Rhode, W.
Ribordy, M.
Richman, M.
Riedel, B.
Rodrigues, J. P.
Rothmaier, F.
Rott, C.
Ruhe, T.
Ruzybayev, B.
Ryckbosch, D.
Saba, S. M.
Salameh, T.
Sander, H. -G.
Santander, M.
Sarkar, S.
Schatto, K.
Scheel, M.
Scheriau, F.
Schmidt, T.
Schmitz, M.
Schoenen, S.
Schoeneberg, S.
Schoenherr, L.
Schoenwald, A.
Schukraft, A.
Schulte, L.
Schulz, O.
Seckel, D.
Seo, S. H.
Sestayo, Y.
Seunarine, S.
Sheremata, C.
Smith, M. W. E.
Soiron, M.
Soldin, D.
Spiczak, G. M.
Spiering, C.
Stamatikos, M.
Stanev, T.
Stasik, A.
Stezelberger, T.
Stokstad, R. G.
Stoessl, A.
Strahler, E. A.
Strom, R.
Sullivan, G. W.
Taavola, H.
Taboada, I.
Tamburro, A.
Ter-Antonyan, S.
Tilav, S.
Toale, P. A.
Toscano, S.
Usner, M.
van der Drift, D.
van Eijndhoven, N.
Van Overloop, A.
van Santen, J.
Vehring, M.
Voge, M.
Vraeghe, M.
Walck, C.
Waldenmaier, T.
Wallraff, M.
Walter, M.
Wasserman, R.
Weaver, Ch.
Wendt, C.
Westerhoff, S.
Whitehorn, N.
Wiebe, K.
Wiebusch, C. H.
Williams, D. R.
Wissing, H.
Wolf, M.
Wood, T. R.
Woschnagg, K.
Xu, C.
Xu, D. L.
Xu, X. W.
Yanez, J. P.
Yodh, G.
Yoshida, S.
Zarzhitsky, P.
Ziemann, J.
Zierke, S.
Zilles, A.
Zoll, M.
CA IceCube Collaboration
TI Search for Galactic PeV gamma rays with the IceCube Neutrino Observatory
SO PHYSICAL REVIEW D
LA English
DT Article
ID MOLECULAR CLOUDS; HESS; DISCOVERY; EMISSION; TEV; PLANE; TELESCOPE;
RADIATION; MILAGRO
AB Gamma-ray induced air showers are notable for their lack of muons, compared to hadronic showers. Hence, air shower arrays with large underground muon detectors can select a sample greatly enriched in photon showers by rejecting showers containing muons. IceCube is sensitive to muons with energies above similar to 500 GeV at the surface, which provides an efficient veto system for hadronic air showers with energies above 1 PeV. One year of data from the 40-string IceCube configuration was used to perform a search for point sources and a Galactic diffuse signal. No sources were found, resulting in a 90% C.L. upper limit on the ratio of gamma rays to cosmic rays of 1.2 x 10(-3) for the flux coming from the Galactic plane region (-80 degrees less than or similar to l less than or similar to -30 degrees; -10 degrees less than or similar to b less than or similar to 5 degrees) in the energy range 1.2-6.0 PeV. In the same energy range, point source fluxes with E-2 spectra have been excluded at a level of (E/TeV)(2)d Phi/dE similar to 10(-12)-10(-11) cm(-2) s(-1) TeV-1 depending on source declination. The complete IceCube detector will have a better sensitivity (due to the larger detector size), improved reconstruction, and vetoing techniques. Preliminary data from the nearly final IceCube detector configuration have been used to estimate the 5-yr sensitivity of the full detector. It is found to be more than an order of magnitude better, allowing the search for PeV extensions of known TeV gamma-ray emitters. DOI: 10.1103/PhysRevD.87.062002
C1 [Bissok, M.; Blumenthal, J.; Boersma, D. J.; Euler, S.; Heimann, P.; Heinen, D.; Paul, L.; Raedel, L.; Scheel, M.; Schoenen, S.; Schoenherr, L.; Schukraft, A.; Soiron, M.; Vehring, M.; Wallraff, M.; Wiebusch, C. H.; Zierke, S.; Zilles, A.] Rhein Westfal TH Aachen, Inst Phys 3, D-52056 Aachen, Germany.
[Aartsen, M. G.; Hill, G. C.] Univ Adelaide, Sch Chem & Phys, Adelaide, SA 5005, Australia.
[Rawlins, K.] Univ Alaska Anchorage, Dept Phys & Astron, Anchorage, AK 99508 USA.
[Japaridze, G. S.] Clark Atlanta Univ, CTSPS, Atlanta, GA 30314 USA.
[Casey, J.; Daughhetee, J.; Taboada, I.] Georgia Inst Technol, Sch Phys, Atlanta, GA 30332 USA.
[Casey, J.; Daughhetee, J.; Taboada, I.] Georgia Inst Technol, Ctr Relativist Astrophys, Atlanta, GA 30332 USA.
[Fazely, A. R.; Ter-Antonyan, S.; Xu, X. W.] Southern Univ, Dept Phys, Baton Rouge, LA 70813 USA.
[Bay, R.; Filimonov, K.; Gerhardt, L.; Ha, C.; Klein, S. R.; Miarecki, S.; Price, P. B.; van der Drift, D.; Woschnagg, K.] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA.
[Beattie, K.; Gerhardt, L.; Goldschmidt, A.; Ha, C.; Klein, S. R.; Matis, H. S.; Miarecki, S.; Nygren, D. R.; Przybylski, G. T.; Stezelberger, T.; Stokstad, R. G.; van der Drift, D.] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Berkeley, CA 94720 USA.
[Altmann, D.; Kappes, A.; Kolanoski, H.; Waldenmaier, T.] Humboldt Univ, Inst Phys, D-12489 Berlin, Germany.
[Tjus, J. Becker; Dreyer, J.; Fedynitch, A.; Olivo, M.; Saba, S. M.; Schoeneberg, S.] Ruhr Univ Bochum, Fak Phys & Astron, D-44780 Bochum, Germany.
[Boeser, S.; Franckowiak, A.; Homeier, A.; Kowalski, M.; Panknin, S.; Schulte, L.; Stasik, A.; Usner, M.; Voge, M.] Univ Bonn, Inst Phys, D-53115 Bonn, Germany.
[Bechet, S.; Bertrand, D.; Hanson, K.; Heereman, D.; Meures, T.; O'Murchadha, A.] Univ Libre Brussels, Sci Fac CP230, B-1050 Brussels, Belgium.
[Bose, D.; Brayeur, L.; Buitink, S.; Casier, M.; De Clercq, C.; Golup, G.; Kunnen, J.; Labare, M.; Miller, J.; Strahler, E. A.; van Eijndhoven, N.] Vrije Univ Brussel, Dienst ELEM, B-1050 Brussels, Belgium.
[Ishihara, A.; Mase, K.; Yoshida, S.] Chiba Univ, Dept Phys, Chiba 2638522, Japan.
[Adams, J.; Brown, A. M.; Hickford, S.] Univ Canterbury, Dept Phys & Astron, Christchurch 1, New Zealand.
[Berley, D.; Blaufuss, E.; Christy, B.; Ellsworth, R. W.; Goodman, J. A.; Hellauer, R.; Hoffman, K. D.; Huelsnitz, W.; Meagher, K.; Olivas, A.; Redl, P.; Richman, M.; Schmidt, T.; Sullivan, G. W.; Wissing, H.] Univ Maryland, Dept Phys, College Pk, MD 20742 USA.
[Beatty, J. J.; Davis, J. C.; Rott, C.; Stamatikos, M.] Ohio State Univ, Dept Phys, Columbus, OH 43210 USA.
[Beatty, J. J.; Davis, J. C.; Rott, C.; Stamatikos, M.] Ohio State Univ, Ctr Cosmol & Astroparticle Phys, Columbus, OH 43210 USA.
[Beatty, J. J.] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA.
[Clevermann, F.; Frantzen, K.; Fuchs, T.; Koehne, J-H.; Milke, N.; Pieloth, D.; Rhode, W.; Ruhe, T.; Scheriau, F.; Schmitz, M.; Ziemann, J.] TU Dortmund Univ, Dept Phys, D-44221 Dortmund, Germany.
[Bohaichuk, S.; Grant, D.; Nowicki, S. C.; Sheremata, C.; Wood, T. R.] Univ Alberta, Dept Phys, Edmonton, AB T6G 2G7, Canada.
[Aguilar, J. A.; Montaruli, T.] Univ Geneva, Dept Phys Nucl & Corpusculaire, CH-1211 Geneva, Switzerland.
[Abdou, Y.; Carson, M.; De Ridder, S.; de Vries-Uiterweerd, G.; Feusels, T.; Ismail, A. Haj; Jlelati, O.; Ryckbosch, D.; Van Overloop, A.; Vraeghe, M.] Univ Ghent, Dept Phys & Astron, B-9000 Ghent, Belgium.
[Barwick, S. W.; Yodh, G.] Univ Calif Irvine, Dept Phys & Astron, Irvine, CA 92697 USA.
[Bruijn, R.; Cohen, S.; Ribordy, M.] Ecole Polytech Fed Lausanne, High Energy Phys Lab, CH-1015 Lausanne, Switzerland.
[Besson, D. Z.] Univ Kansas, Dept Phys & Astron, Lawrence, KS 66045 USA.
[Gallagher, J.] Univ Wisconsin, Dept Astron, Madison, WI 53706 USA.
[Abbasi, R.; Ahlers, M.; Andeen, K.; Auffenberg, J.; Baker, M.; BenZvi, S.; Chirkin, D.; Descamps, F.; Desiati, P.; Diaz-Velez, J. C.; Dumm, J. P.; Eisch, J.; Fadiran, O.; Feintzeig, J.; Gladstone, L.; Grullon, S.; Halzen, F.; Hoshina, K.; Jacobsen, J.; Karle, A.; Kopper, C.; Krasberg, M.; Kurahashi, N.; Landsman, H.; Maruyama, R.; McNally, F.; Merck, M.; Morse, R.; Riedel, B.; Rodrigues, J. P.; Santander, M.; Toscano, S.; van Santen, J.; Weaver, Ch.; Wendt, C.; Westerhoff, S.; Whitehorn, N.] Univ Wisconsin, Dept Phys, Madison, WI 53706 USA.
[Abbasi, R.; Ahlers, M.; Andeen, K.; Auffenberg, J.; Baker, M.; BenZvi, S.; Chirkin, D.; Descamps, F.; Desiati, P.; Diaz-Velez, J. C.; Dumm, J. P.; Eisch, J.; Fadiran, O.; Feintzeig, J.; Gladstone, L.; Grullon, S.; Halzen, F.; Hoshina, K.; Jacobsen, J.; Karle, A.; Kopper, C.; Krasberg, M.; Kurahashi, N.; Landsman, H.; Maruyama, R.; McNally, F.; Merck, M.; Morse, R.; Riedel, B.; Rodrigues, J. P.; Santander, M.; Toscano, S.; van Santen, J.; Weaver, Ch.; Wendt, C.; Westerhoff, S.; Whitehorn, N.] Univ Wisconsin, Wisconsin IceCube Particle Astrophys Ctr, Madison, WI 53706 USA.
[Baum, V.; Koepke, L.; Kroll, G.; Luenemann, J.; Rothmaier, F.; Sander, H. -G.; Schatto, K.; Wiebe, K.] Johannes Gutenberg Univ Mainz, Inst Phys, D-55099 Mainz, Germany.
[Kohnen, G.] Univ Mons, B-7000 Mons, Belgium.
[Gross, A.; Odrowski, S.; Resconi, E.; Schulz, O.; Sestayo, Y.] Tech Univ Munich, D-85748 Garching, Germany.
[Bai, X.; Evenson, P. A.; Gaisser, T. K.; Hussain, S.; Kuwabara, T.; Ruzybayev, B.; Seckel, D.; Stanev, T.; Tamburro, A.; Tilav, S.; Xu, C.] Univ Delaware, Bartol Res Inst, Newark, DE 19716 USA.
[Bai, X.; Evenson, P. A.; Gaisser, T. K.; Hussain, S.; Kuwabara, T.; Ruzybayev, B.; Seckel, D.; Stanev, T.; Tamburro, A.; Tilav, S.; Xu, C.] Univ Delaware, Dept Phys & Astron, Newark, DE 19716 USA.
[Sarkar, S.] Univ Oxford, Dept Phys, Oxford OX1 3NP, England.
[Madsen, J.; Seunarine, S.; Spiczak, G. M.] Univ Wisconsin, Dept Phys, River Falls, WI 54022 USA.
[Bohm, C.; Danninger, M.; Finley, C.; Flis, S.; Hulth, P. O.; Hultqvist, K.; Seo, S. H.; Walck, C.; Wolf, M.; Zoll, M.] Stockholm Univ, Oskar Klein Ctr, SE-10691 Stockholm, Sweden.
[Bohm, C.; Danninger, M.; Finley, C.; Flis, S.; Hulth, P. O.; Hultqvist, K.; Seo, S. H.; Walck, C.; Wolf, M.; Zoll, M.] Stockholm Univ, Dept Phys, SE-10691 Stockholm, Sweden.
[Kiryluk, J.; Lesiak-Bzdak, M.] SUNY Stony Brook, Dept Phys & Astron, Stony Brook, NY 11794 USA.
[Larson, M. J.; Pepper, J. A.; Toale, P. A.; Williams, D. R.; Xu, D. L.; Zarzhitsky, P.] Univ Alabama, Dept Phys & Astron, Tuscaloosa, AL 35487 USA.
[Cowen, D. F.; Meszaros, P.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA.
[Bell, M.; Clark, K.; Cowen, D. F.; DeYoung, T.; Dunkman, M.; Eagan, R.; Koskinen, D. J.; Meszaros, P.; Salameh, T.; Smith, M. W. E.; Wasserman, R.] Penn State Univ, Dept Phys, University Pk, PA 16802 USA.
[Boersma, D. J.; Botner, O.; Engdegard, O.; Hallgren, A.; de los Heros, C. Perez; Strom, R.; Taavola, H.] Uppsala Univ, Dept Phys & Astron, S-75120 Uppsala, Sweden.
[Becker, K. -H.; Bindig, D.; Fischer-Wasels, T.; Gurtner, M.; Helbing, K.; Hoffmann, R.; Klaes, J.; Kopper, S.; Naumann, U.; Obertacke, A.; Posselt, J.; Soldin, D.] Univ Wuppertal, Dept Phys, D-42119 Wuppertal, Germany.
[Ackermann, M.; Benabderrahmane, M. L.; Berdermann, J.; Berghaus, P.; Bernardini, E.; Brunner, J.; Silva, A. H. Cruz; Franke, R.; Gluesenkamp, T.; Gora, D.; Jacobi, E.; Karg, T.; Kislat, F.; Lauer, R.; Middell, E.; Mohrmann, L.; Nahnhauer, R.; Pirk, N.; Schoenwald, A.; Spiering, C.; Stoessl, A.; Walter, M.; Yanez, J. P.] DESY, D-15735 Zeuthen, Germany.
[Bai, X.] South Dakota Sch Mines & Technol, Dept Phys, Rapid City, SD 57701 USA.
[Buitink, S.] Univ Groningen, KVI, NL-9747 AA Groningen, Netherlands.
[Huelsnitz, W.] Los Alamos Natl Lab, Los Alamos, NM 87545 USA.
[Montaruli, T.] Sezione Ist Nazl Fis Nucl, Dipartimento Fis, I-70126 Bari, Italy.
[Stamatikos, M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Buitink, S (reprint author), Vrije Univ Brussel, Dienst ELEM, B-1050 Brussels, Belgium.
EM s.j.buitink@rug.nl
RI Taavola, Henric/B-4497-2011; Sarkar, Subir/G-5978-2011; Tjus,
Julia/G-8145-2012; Wiebusch, Christopher/G-6490-2012; Auffenberg,
Jan/D-3954-2014; Koskinen, David/G-3236-2014; Brunner,
Juergen/G-3540-2015; Aguilar Sanchez, Juan Antonio/H-4467-2015;
Maruyama, Reina/A-1064-2013; Beatty, James/D-9310-2011;
OI Taavola, Henric/0000-0002-2604-2810; Buitink, Stijn/0000-0002-6177-497X;
Carson, Michael/0000-0003-0400-7819; Perez de los Heros,
Carlos/0000-0002-2084-5866; Benabderrahmane, Mohamed
Lotfi/0000-0003-4410-5886; Ter-Antonyan, Samvel/0000-0002-5788-1369;
Schukraft, Anne/0000-0002-9112-5479; Sarkar, Subir/0000-0002-3542-858X;
Wiebusch, Christopher/0000-0002-6418-3008; Auffenberg,
Jan/0000-0002-1185-9094; Koskinen, David/0000-0002-0514-5917; Brunner,
Juergen/0000-0002-5052-7236; Aguilar Sanchez, Juan
Antonio/0000-0003-2252-9514; Maruyama, Reina/0000-0003-2794-512X;
Beatty, James/0000-0003-0481-4952; Rott, Carsten/0000-0002-6958-6033
FU U.S. National Science Foundation-Office of Polar Programs; U.S. National
Science Foundation-Physics Division; University of Wisconsin Alumni
Research Foundation; Grid Laboratory Of Wisconsin (GLOW) grid
infrastructure at the University of Wisconsin-Madison; Open Science Grid
(OSG) grid infrastructure; U.S. Department of Energy, and National
Energy Research Scientific Computing Center; Louisiana Optical Network
Initiative (LONI) grid computing resources; National Science and
Engineering Research Council of Canada; Swedish Research Council;
Swedish Polar Research Secretariat; Swedish National Infrastructure for
Computing (SNIC); Knut and Alice Wallenberg Foundation, Sweden; German
Ministry for Education and Research (BMBF); Deutsche
Forschungsgemeinschaft (DFG); Research Department of Plasmas with
Complex Interactions (Bochum), Germany; Fund for Scientific Research
(FNRS-FWO); FWO Odysseus programme; Flanders Institute to encourage
scientific and technological research in industry (IWT); Belgian Federal
Science Policy Office (Belspo); University of Oxford, United Kingdom;
Marsden Fund, New Zealand; Australian Research Council; Japan Society
for Promotion of Science (JSPS); Swiss National Science Foundation
(SNSF), Switzerland
FX We acknowledge the support from the following agencies: U.S. National
Science Foundation-Office of Polar Programs, U.S. National Science
Foundation-Physics Division, University of Wisconsin Alumni Research
Foundation, the Grid Laboratory Of Wisconsin (GLOW) grid infrastructure
at the University of Wisconsin-Madison, the Open Science Grid (OSG) grid
infrastructure; U.S. Department of Energy, and National Energy Research
Scientific Computing Center, the Louisiana Optical Network Initiative
(LONI) grid computing resources; National Science and Engineering
Research Council of Canada; Swedish Research Council, Swedish Polar
Research Secretariat, Swedish National Infrastructure for Computing
(SNIC), and Knut and Alice Wallenberg Foundation, Sweden; German
Ministry for Education and Research (BMBF), Deutsche
Forschungsgemeinschaft (DFG), Research Department of Plasmas with
Complex Interactions (Bochum), Germany; Fund for Scientific Research
(FNRS-FWO), FWO Odysseus programme, Flanders Institute to encourage
scientific and technological research in industry (IWT), Belgian Federal
Science Policy Office (Belspo); University of Oxford, United Kingdom;
Marsden Fund, New Zealand; Australian Research Council; Japan Society
for Promotion of Science (JSPS); and the Swiss National Science
Foundation (SNSF), Switzerland.
NR 37
TC 21
Z9 21
U1 1
U2 16
PU AMER PHYSICAL SOC
PI COLLEGE PK
PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA
SN 1550-7998
J9 PHYS REV D
JI Phys. Rev. D
PD MAR 20
PY 2013
VL 87
IS 6
AR 062002
DI 10.1103/PhysRevD.87.062002
PG 15
WC Astronomy & Astrophysics; Physics, Particles & Fields
SC Astronomy & Astrophysics; Physics
GA 110CB
UT WOS:000316418600002
ER
PT J
AU Podio, L
Kamp, I
Codella, C
Cabrit, S
Nisini, B
Dougados, C
Sandell, G
Williams, JP
Testi, L
Thi, WF
Woitke, P
Meijerink, R
Spaans, M
Aresu, G
Menard, F
Pinte, C
AF Podio, L.
Kamp, I.
Codella, C.
Cabrit, S.
Nisini, B.
Dougados, C.
Sandell, G.
Williams, J. P.
Testi, L.
Thi, W. -F.
Woitke, P.
Meijerink, R.
Spaans, M.
Aresu, G.
Menard, F.
Pinte, C.
TI WATER VAPOR IN THE PROTOPLANETARY DISK OF DG Tau
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE astrochemistry; ISM: molecules; protoplanetary disks; stars: individual
(DG Tau)
ID CIRCUMSTELLAR DISKS; CONTINUUM EMISSION; STARS; HERSCHEL; LINE;
SUBMILLIMETER; SYSTEM; GAS; JET; I.
AB Water is key in the evolution of protoplanetary disks and the formation of comets and icy/water planets. While high-excitation water lines originating in the hot inner disk have been detected in several T Tauri stars (TTSs), water vapor from the outer disk, where most water ice reservoirs are stored, was only reported in the nearby TTS TW Hya. We present spectrally resolved Herschel/HIFI observations of the young TTS DG Tau in the ortho-and para-water ground-state transitions at 557 and 1113 GHz. The lines show a narrow double-peaked profile, consistent with an origin in the outer disk, and are similar to 19-26 times brighter than in TW Hya. In contrast, CO and [C II] lines are dominated by emission from the envelope/outflow, which makes H2O lines a unique tracer of the disk of DG Tau. Disk modeling with the thermo-chemical code ProDiMo indicates that the strong UV field, due to the young age and strong accretion of DG Tau, irradiates a disk upper layer at 10-90 AU from the star, heating it up to temperatures of 600 K and producing the observed bright water lines. The models suggest a disk mass of 0.015-0.1 M-circle dot, consistent with the estimated minimum mass of the solar nebula before planet formation, and a water reservoir of similar to 10(2)-10(3) Earth oceans in vapor and similar to 100 times larger in the form of ice. Hence, this detection supports the scenario of ocean delivery on terrestrial planets by the impact of icy bodies forming in the outer disk.
C1 [Podio, L.; Dougados, C.; Thi, W. -F.; Menard, F.; Pinte, C.] UJF Grenoble 1 CNRS INSU, IPAG UMR 5274, F-38041 Grenoble, France.
[Kamp, I.; Meijerink, R.; Spaans, M.; Aresu, G.] Univ Groningen, Kapteyn Astron Inst, NL-9747 AD Groningen, Netherlands.
[Codella, C.] INAF Osservatorio Astrofis Arcetri, I-50125 Florence, Italy.
[Cabrit, S.] Univ Cergy Pontoise, Univ Paris 06, Ecole Normale Super, Observ Paris,UMR CNR 8112,LERMA, F-75014 Paris, France.
[Nisini, B.] INAF Osservatorio Astron Roma, I-00040 Monte Porzio Catone, Italy.
[Dougados, C.; Menard, F.] Univ Chile, LFCA, CNRS, UMI 3386, Santiago, Chile.
[Dougados, C.; Menard, F.] Univ Chile, Dept Astron, Santiago, Chile.
[Sandell, G.] NASA, Ames Res Ctr, SOFIA USRA, Moffett Field, CA 94035 USA.
[Williams, J. P.] Univ Hawaii, Inst Astron IfA, Honolulu, HI 96822 USA.
[Testi, L.] European So Observ, D-85748 Garching, Germany.
[Woitke, P.] Univ St Andrews, SUPA, Sch Phys & Astron, St Andrews KY16 9SS, Fife, Scotland.
RP Podio, L (reprint author), UJF Grenoble 1 CNRS INSU, IPAG UMR 5274, F-38041 Grenoble, France.
OI Meijerink, Rowin/0000-0001-7584-9293; Williams,
Jonathan/0000-0001-5058-695X; Codella, Claudio/0000-0003-1514-3074; ,
Brunella Nisini/0000-0002-9190-0113
FU European 7th Framework Program (FP7) [PIEF-GA-2009-253896,
PERG06-GA-2009-256513]; Agence Nationale pour la Recherche (ANR)
[ANR-2010-JCJC-0504-01]; FP7-2011 [284405]; Service Commun de Calcul
Intensif de l'IPAG [ANR-2010-JCJC-0504-01, ANR-07-BLAN-0221,
ANR-2010-JCJC-0501-01]
FX L.P. and C.P. acknowledge funding from the European 7th Framework
Program (FP7; contracts PIEF-GA-2009-253896 and PERG06-GA-2009-256513),
and from Agence Nationale pour la Recherche (ANR; contract
ANR-2010-JCJC-0504-01). We also acknowledge funding from FP7-2011
(contract 284405), and the Service Commun de Calcul Intensif de l'IPAG
for computations (contracts ANR-07-BLAN-0221, ANR-2010-JCJC-0504-01, and
ANR-2010-JCJC-0501-01).
NR 36
TC 17
Z9 17
U1 0
U2 6
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 2041-8205
J9 ASTROPHYS J LETT
JI Astrophys. J. Lett.
PD MAR 20
PY 2013
VL 766
IS 1
AR L5
DI 10.1088/2041-8205/766/1/L5
PG 5
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 103WH
UT WOS:000315949700005
ER
PT J
AU Trainer, MG
Sebree, JA
Yoon, YH
Tolbert, MA
AF Trainer, Melissa G.
Sebree, Joshua A.
Yoon, Y. Heidi
Tolbert, Margaret A.
TI THE INFLUENCE OF BENZENE AS A TRACE REACTANT IN TITAN AEROSOL ANALOGS
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE planets and satellites: atmospheres; planets and satellites: individual
(Titan)
ID POLYCYCLIC AROMATIC-HYDROCARBONS; PHOTOABSORPTION CROSS-SECTIONS;
UPPER-ATMOSPHERE; MASS-SPECTROMETER; HIGH-RESOLUTION; PHOTODISSOCIATION;
CHEMISTRY; METHANE; THERMOSPHERE; KINETICS
AB Benzene has been detected in Titan's atmosphere by Cassini instruments, with concentrations ranging from sub-ppb in the stratosphere to ppm in the ionosphere. Sustained levels of benzene in the haze formation region could signify that it is an important reactant in the formation of Titan's organic aerosol. To date, there have not been laboratory investigations to assess the influence of benzene on aerosol properties. We report a laboratory study on the chemical composition of organic aerosol formed from C6H6/CH4/N-2 via far ultraviolet irradiation (120-200 nm). The compositional results are compared to those from aerosol generated by a more "traditional Titan" mixture of CH4/N-2. Our results show that even a trace amount of C6H6 (10 ppm) has significant impact on the chemical composition and production rates of organic aerosol. There are several pathways by which photolyzed benzene may react to form larger molecules, both with and without the presence of CH4, but many of these reaction mechanisms are only beginning to be explored for the conditions at Titan. Continued work investigating the influence of benzene in aerosol growth will advance understanding of this previously unstudied reaction system.
C1 [Trainer, Melissa G.] NASA, Goddard Space Flight Ctr, Planetary Environm Lab, Greenbelt, MD 20771 USA.
[Sebree, Joshua A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Yoon, Y. Heidi; Tolbert, Margaret A.] Univ Colorado, Cooperat Inst Res Environm Sci, Boulder, CO 80309 USA.
[Tolbert, Margaret A.] Univ Colorado, Dept Chem & Biochem, Boulder, CO 80309 USA.
RP Trainer, MG (reprint author), NASA, Goddard Space Flight Ctr, Planetary Environm Lab, Code 699, Greenbelt, MD 20771 USA.
EM melissa.trainer@nasa.gov
RI Trainer, Melissa/E-1477-2012
FU National Aeronautics and Space Administration [NNX11AD82G,
10-PATM10-0027]; Goddard Space Flight Center; NASA; CIRES; National
Oceanic and Atmospheric Administration
FX The authors thank C. M. Anderson for the Titan vertical aerosol profile.
This material is based upon work supported by the National Aeronautics
and Space Administration under grants NNX11AD82G and 10-PATM10-0027
issued through the Planetary Atmospheres Program. J.A.S. was supported
by an appointment to the NASA Postdoctoral Program at the Goddard Space
Flight Center, administered by Oak Ridge Associated Universities through
a contract with NASA. Y.H.Y. was supported by the CIRES Visiting Fellows
Program, sponsored by the National Oceanic and Atmospheric
Administration.
NR 28
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U1 3
U2 26
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 2041-8205
EI 2041-8213
J9 ASTROPHYS J LETT
JI Astrophys. J. Lett.
PD MAR 20
PY 2013
VL 766
IS 1
AR L4
DI 10.1088/2041-8205/766/1/L4
PG 5
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 103WH
UT WOS:000315949700004
ER
PT J
AU Knyazikhin, Y
Lewis, P
Disney, MI
Stenberg, P
Mottus, M
Rautiainen, M
Kaufmann, RK
Marshak, A
Schull, MA
Carmona, PL
Vanderbilt, V
Davis, AB
Baret, F
Jacquemoud, S
Lyapustin, A
Yang, Y
Myneni, RB
AF Knyazikhin, Yuri
Lewis, Philip
Disney, Mathias I.
Stenberg, Pauline
Mottus, Matti
Rautiainen, Miina
Kaufmann, Robert K.
Marshak, Alexander
Schull, Mitchell A.
Latorre Carmona, Pedro
Vanderbilt, Vern
Davis, Anthony B.
Baret, Frederic
Jacquemoud, Stephane
Lyapustin, Alexei
Yang, Yan
Myneni, Ranga B.
TI Reply toTownsend et al.: Decoupling contributions from canopy structure
and leaf optics is critical for remote sensing leaf biochemistry
SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF
AMERICA
LA English
DT Letter
ID NITROGEN; ALBEDO
C1 [Knyazikhin, Yuri; Kaufmann, Robert K.; Yang, Yan; Myneni, Ranga B.] Boston Univ, Dept Earth & Environm, Boston, MA 02215 USA.
[Lewis, Philip; Disney, Mathias I.] UCL, Dept Geog, London WC1E 6BT, England.
[Lewis, Philip; Disney, Mathias I.] UCL, Natl Ctr Earth Observat, London WC1E 6BT, England.
[Stenberg, Pauline; Rautiainen, Miina] Univ Helsinki, Dept Forest Sci, FI-00014 Helsinki, Finland.
[Mottus, Matti] Univ Helsinki, Dept Geosci & Geog, FI-00014 Helsinki, Finland.
[Marshak, Alexander; Lyapustin, Alexei] NASA, Goddard Space Flight Ctr, Climate & Radiat Lab, Greenbelt, MD 20771 USA.
[Schull, Mitchell A.] USDA ARS, Hydrol & Remote Sensing Lab, Beltsville, MD USA.
[Latorre Carmona, Pedro] Univ Jaume 1, Dept Lenguajes & Sistemas Informat, Castellon de La Plana 12071, Spain.
[Vanderbilt, Vern] NASA, Ames Res Ctr, Biospher Sci Branch, Div Earth Sci, Moffett Field, CA 94035 USA.
[Davis, Anthony B.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Baret, Frederic] Inst Natl Rech Agronom Site Agroparc, Unite Mixte Rech Environm Mediterraneen & Modelis, F-84914 Avignon, France.
[Jacquemoud, Stephane] Univ Paris Diderot, Unite Mixte Rech, Ctr Natl Rech Sci, Inst Phys Globe Paris Sorbonne Paris Cite, F-75013 Paris, France.
RP Knyazikhin, Y (reprint author), Boston Univ, Dept Earth & Environm, Boston, MA 02215 USA.
EM jknjazi@bu.edu
RI Disney, Mathias/C-1889-2008; Rautiainen, Miina/A-4208-2009; Mottus,
Matti/A-4130-2009; Marshak, Alexander/D-5671-2012; Lyapustin,
Alexei/H-9924-2014; Myneni, Ranga/F-5129-2012; Baret, Fred/C-4135-2011;
Jacquemoud, Stephane/F-8842-2010
OI Rautiainen, Miina/0000-0002-6568-3258; Mottus,
Matti/0000-0002-2745-1966; Lyapustin, Alexei/0000-0003-1105-5739; Baret,
Fred/0000-0002-7655-8997;
NR 4
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U1 2
U2 28
PU NATL ACAD SCIENCES
PI WASHINGTON
PA 2101 CONSTITUTION AVE NW, WASHINGTON, DC 20418 USA
SN 0027-8424
J9 P NATL ACAD SCI USA
JI Proc. Natl. Acad. Sci. U. S. A.
PD MAR 19
PY 2013
VL 110
IS 12
BP E1075
EP E1075
DI 10.1073/pnas.1301247110
PG 1
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 125EK
UT WOS:000317521600002
PM 23630977
ER
PT J
AU Schmerr, NC
Kelly, BM
Thorne, MS
AF Schmerr, Nicholas C.
Kelly, Byron M.
Thorne, Michael S.
TI Broadband array observations of the 300km seismic discontinuity
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
DE 300 km discontinuity; SS and PP precursors; basalt; eclogite; wave
propagation; High Lava Plains Seismic Experiment; EarthScope
ID UPPER-MANTLE; SS-PRECURSORS; REFLECTIVITY; SUBDUCTION; MIGRATION;
VELOCITY; MODEL; EARTH
AB Intermittent seismic discontinuities near 250-300 km depth beneath South America and the Pacific basin are detected with high-resolution seismic array methods that use SS and PP precursors recorded at the High Lava Plains Seismic Experiment and the EarthScope Transportable Array. The transformation of coesite to stishovite in an eclogite-rich mantle composition produces a seismic discontinuity near 300 km depth; lateral changes in basalt fraction of the upper mantle will thus produce an intermittent seismic discontinuity. The sensitivity of the precursors to intermittent seismic structure is addressed using an axisymmetric finite difference model of wave propagation in the mantle. These numerical experiments find that the precursors are sensitive to structures >= 500 km in lateral extent and that the observations of this discontinuity are plausibly tied to lateral variations in basaltic composition of the upper mantle related to dynamics, such as plumes and subduction. Citation: Schmerr, N. C., B. M. Kelly, and M. S. Thorne (2013), Broadband array observations of the 300 km seismic discontinuity, Geophys. Res. Lett., 40, 841-846, doi:10.1002/grl.50257.
C1 [Schmerr, Nicholas C.] NASA, Goddard Space Flight Ctr, Planetary Geodynam Lab, Greenbelt, MD 20771 USA.
[Kelly, Byron M.] Univ Calgary, Dept Geosci, Calgary, AB, Canada.
[Thorne, Michael S.] Univ Utah, Dept Geol & Geophys, Salt Lake City, UT 84112 USA.
RP Schmerr, NC (reprint author), NASA, Goddard Space Flight Ctr, Planetary Geodynam Lab, Code 698, Greenbelt, MD 20771 USA.
EM nicholas.c.schmerr@nasa.gov
OI Schmerr, Nicholas/0000-0002-3256-1262
FU NASA; Carnegie Institution of Washington Summer Scholars Program;
University of Utah Center for High Performance Computing (CHPC);
National Science Foundation [EAR-0952187]
FX The authors thank two anonymous reviewers and the editor, Michael
Wysession, for constructive comments that helped to improve the quality
of the manuscript. Data were collected with Standing Order for Data
[Owens et al., 2004] and EMERALD [West and Fouch, 2012] software. Data
analyses were performed using TauP [Crotwell et al., 1999] and Seismic
Analysis Code [Goldstein et al., 2003]. Figures were generated using GMT
[Wessel and Smith, 1998]. NS was supported by a NASA Postdoctoral
Program Fellowship. BK was supported by the Carnegie Institution of
Washington Summer Scholars Program. The authors gratefully acknowledge
the University of Utah Center for High Performance Computing (CHPC) for
computer resources and support. MT was partially supported by the
National Science Foundation (grant no. EAR-0952187).
NR 35
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U1 0
U2 16
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0094-8276
EI 1944-8007
J9 GEOPHYS RES LETT
JI Geophys. Res. Lett.
PD MAR 16
PY 2013
VL 40
IS 5
BP 841
EP 846
DI 10.1002/grl.50257
PG 6
WC Geosciences, Multidisciplinary
SC Geology
GA 134VG
UT WOS:000318242900008
ER
PT J
AU Wei, SJ
Helmberger, D
Owen, S
Graves, RW
Hudnut, KW
Fielding, EJ
AF Wei, Shengji
Helmberger, Don
Owen, Susan
Graves, Robert W.
Hudnut, Kenneth W.
Fielding, Eric J.
TI Complementary slip distributions of the largest earthquakes in the 2012
Brawley swarm, Imperial Valley, California
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
DE Brawley Earthquake Swarm Imperial Valley; high-rate GPS; geothermal;
strong motion
ID SOUTHERN CALIFORNIA; MODEL; FAULT; EVENTS
AB We investigate the finite rupture processes of two M>5 earthquakes in the 2012 Brawley swarm by joint inversion of nearby strong motion and high-rate GPS data. Waveform inversions up to 3 Hz were made possible by using a small event (Mw3.9) for path calibration of the velocity structure. Our results indicate that the first (Mw5.3) event ruptured a strong, concentrated asperity with offsets of similar to 20 cm centered at a depth of 5 km. The subsequent Mw5.4 event occurred 1.5 h later with a shallower slip distribution that surrounds and is complementary to that of the earlier event. The second event has a longer rise time and weaker high-frequency energy release compared to the Mw5.3 event. Both events display strong rupture directivity toward the southwest and lack of very shallow (<2 km) coseismic slip. The hypocenters for these events appear to be near or in the bedrock, but most of the slip is distributed at shallower depths (<6 km) and can explain a large part of the GPS offsets for the swarm. The complementary slip distributions of the two events suggest a triggering relationship between them with no significant creep needed to explain the various data sets.
C1 [Wei, Shengji; Helmberger, Don] CALTECH, Pasadena, CA 91125 USA.
[Owen, Susan; Fielding, Eric J.] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
[Graves, Robert W.; Hudnut, Kenneth W.] US Geol Survey, Pasadena, CA 91106 USA.
RP Wei, SJ (reprint author), CALTECH, Pasadena, CA 91125 USA.
EM shjwei@gmail.com
RI Hudnut, Kenneth/B-1945-2009; Wei, Shengji/M-2137-2015; Fielding,
Eric/A-1288-2007
OI Hudnut, Kenneth/0000-0002-3168-4797; Wei, Shengji/0000-0002-0319-0714;
Fielding, Eric/0000-0002-6648-8067
FU USGS [G12AP20072]; Caltech Tectonics Observatory
FX The strong motion data were downloaded from the Southern California
Seismic Network and USGS. The original TerraSAR-X data is copyright 2012
by the German space agency DLR, provided under the Group on Earth
Observation Geohazard Supersite project. Part of this research was
supported by the USGS grant G12AP20072, Caltech Tectonics Observatory,
NASA Earth Surface and Interior focus area and performed at the JPL,
Caltech. The high-rate GPS data were provided by the NSF PBO and
archived at UNAVCO. Static offset GPS processing was performed by Jerry
Svarc (USGS) and Tom Herring (MIT). The manuscript was improved by the
constructive input of Karen Felzer, Gavin Hayes and two anonymous
reviewers.
NR 30
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U1 0
U2 13
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0094-8276
J9 GEOPHYS RES LETT
JI Geophys. Res. Lett.
PD MAR 16
PY 2013
VL 40
IS 5
BP 847
EP 852
DI 10.1002/grl.50259
PG 6
WC Geosciences, Multidisciplinary
SC Geology
GA 134VG
UT WOS:000318242900009
ER
PT J
AU Hoffman, JS
Carlson, AE
Winsor, K
Klinkhammer, GP
LeGrande, AN
Andrews, JT
Strasser, JC
AF Hoffman, Jeremy S.
Carlson, Anders E.
Winsor, Kelsey
Klinkhammer, Gary P.
LeGrande, Allegra N.
Andrews, John T.
Strasser, Jeffrey C.
TI Linking the 8.2ka event and its freshwater forcing in the Labrador Sea
(vol 39, L18703, 2012)
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Correction
C1 [Hoffman, Jeremy S.; Strasser, Jeffrey C.] Augustana Coll, Dept Geol, Rock Isl, IL 61201 USA.
[Carlson, Anders E.; Winsor, Kelsey] Univ Wisconsin, Dept Geosci, Madison, WI 53706 USA.
[Carlson, Anders E.] Univ Wisconsin, Ctr Climat Res, Madison, WI 53706 USA.
[Carlson, Anders E.; Klinkhammer, Gary P.] Oregon State Univ, Coll Earth Ocean & Atmospher Sci, Corvallis, OR 97331 USA.
[LeGrande, Allegra N.] Columbia Univ, NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
[LeGrande, Allegra N.] Columbia Univ, Ctr Climate Syst Res, New York, NY 10025 USA.
[Andrews, John T.] Univ Colorado, Inst Alpine & Arctic Res, Boulder, CO 80309 USA.
[Andrews, John T.] Univ Colorado, Dept Geol Sci, Boulder, CO 80309 USA.
RP Carlson, AE (reprint author), Oregon State Univ, Coll Earth Ocean & Atmospher Sci, 104 CEOAS Adm Bldg, Corvallis, OR 97331 USA.
NR 2
TC 0
Z9 0
U1 1
U2 3
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0094-8276
J9 GEOPHYS RES LETT
JI Geophys. Res. Lett.
PD MAR 16
PY 2013
VL 40
IS 5
BP 971
EP 971
DI 10.1002/grl.50111
PG 1
WC Geosciences, Multidisciplinary
SC Geology
GA 134VG
UT WOS:000318242900031
ER
PT J
AU Gautam, R
Hsu, NC
Lau, WKM
Yasunari, TJ
AF Gautam, Ritesh
Hsu, N. Christina
Lau, William K.-M.
Yasunari, Teppei J.
TI Satellite observations of desert dust-induced Himalayan snow darkening
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
DE Dust; Snow; Remote Sensing
ID HYDROLOGICAL CYCLE; SPECTRAL ALBEDO; TIBETAN PLATEAU; MONSOON; AEROSOLS;
PRODUCTS; GLACIERS; IMPACTS; CLIMATE; COVER
AB The optically thick aerosol layer along the southern edge of the Himalaya has been subject of several recent investigations relating to its radiative impacts on the South Asian summer monsoon and regional climate forcing. Prior to the onset of summer monsoon, mineral dust from southwest Asian deserts is transported over the Himalayan foothills on an annual basis. Episodic dust plumes are also advected over the Himalaya, visible as dust-laden snow surface in satellite imagery, particularly in western Himalaya. We examined spectral surface reflectance retrieved from spaceborne MODIS observations that show characteristic reduction in the visible wavelengths (0.47 mu m) over western Himalaya, associated with dust-induced solar absorption. Case studies as well as seasonal variations of reflectance indicate a significant gradient across the visible (0.47 mu m) to near-infrared (0.86 mu m) spectrum (VIS-NIR), during premonsoon period. Enhanced absorption at shorter visible wavelengths and the resulting VIS-NIR gradient is consistent with model calculations of snow reflectance with dust impurity. While the role of black carbon in snow cannot be ruled out, our satellite-based analysis suggests the observed spectral reflectance gradient dominated by dust-induced solar absorption during premonsoon season. From an observational viewpoint, this study underscores the importance of mineral dust deposition toward darkening of the western Himalayan snow cover, with potential implications to accelerated seasonal snowmelt and regional snow albedo feedbacks.
C1 [Gautam, Ritesh; Yasunari, Teppei J.] Univ Space Res Assoc, GESTAR, Columbia, MD USA.
[Gautam, Ritesh; Hsu, N. Christina; Lau, William K.-M.; Yasunari, Teppei J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Gautam, R (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
EM Ritesh.Gautam@nasa.gov
RI Hsu, N. Christina/H-3420-2013; Gautam, Ritesh/E-9776-2010; Yasunari,
Teppei/E-5374-2010; Lau, William /E-1510-2012
OI Gautam, Ritesh/0000-0002-2177-9346; Yasunari,
Teppei/0000-0002-9896-9404; Lau, William /0000-0002-3587-3691
FU Terra/Aqua Science Program, NASA Headquarters
FX This work is supported by the Terra/Aqua Science Program, NASA
Headquarters. MODIS science teams are acknowledged for provision of
satellite data. We thank Mark Flanner and Charles Zender for providing
dust optical properties data set, which were used in our snow
reflectance model simulations, and Andrew Sayer for his suggestions and
useful discussions related to snow reflectance modeling. Thomas Painter
and one anonymous reviewer are thanked for helpful comments in improving
an earlier version of the manuscript.
NR 29
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U1 1
U2 41
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0094-8276
J9 GEOPHYS RES LETT
JI Geophys. Res. Lett.
PD MAR 16
PY 2013
VL 40
IS 5
BP 988
EP 993
DI 10.1002/grl.50226
PG 6
WC Geosciences, Multidisciplinary
SC Geology
GA 134VG
UT WOS:000318242900035
ER
PT J
AU Neely, RR
Toon, OB
Solomon, S
Vernier, JP
Alvarez, C
English, JM
Rosenlof, KH
Mills, MJ
Bardeen, CG
Daniel, JS
Thayer, JP
AF Neely, R. R., III
Toon, O. B.
Solomon, S.
Vernier, J. -P.
Alvarez, C.
English, J. M.
Rosenlof, K. H.
Mills, M. J.
Bardeen, C. G.
Daniel, J. S.
Thayer, J. P.
TI Recent anthropogenic increases in SO2 from Asia have minimal impact on
stratospheric aerosol
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
DE Stratosphere; Asian Monsoon; Volcanoes; WACCM
ID EVOLUTION; MODEL; LAYER; ANALOGS
AB Observations suggest that the optical depth of the stratospheric aerosol layer between 20 and 30km has increased 410% per year since 2000, which is significant for Earth's climate. Contributions to this increase both from moderate volcanic eruptions and from enhanced coal burning in Asia have been suggested. Current observations are insufficient to attribute the contribution of the different sources. Here we use a global climate model coupled to an aerosol microphysical model to partition the contribution of each. We employ model runs that include the increases in anthropogenic sulfur dioxide (SO2) over Asia and the moderate volcanic explosive injections of SO2 observed from 2000 to 2010. Comparison of the model results to observations reveals that moderate volcanic eruptions, rather than anthropogenic influences, are the primary source of the observed increases in stratospheric aerosol.
C1 [Neely, R. R., III; Toon, O. B.] Univ Colorado, Dept Atmospher & Ocean Sci, Boulder, CO 80309 USA.
[Neely, R. R., III; Alvarez, C.; Rosenlof, K. H.; Daniel, J. S.] NOAA, Earth Syst Res Lab, Boulder, CO USA.
[Neely, R. R., III; Alvarez, C.] Univ Colorado, NOAA, Cooperat Inst Res Environm Sci, Boulder, CO 80309 USA.
[Toon, O. B.] Univ Colorado, Lab Atmospher & Space Phys, Boulder, CO 80309 USA.
[Solomon, S.] MIT, Dept Earth Atmospher & Planetary Sci, Cambridge, MA USA.
[Vernier, J. -P.] Sci Syst & Applicat Inc, Hampton, VA USA.
[Vernier, J. -P.] NASA, Langley Res Ctr, Hampton, VA 23665 USA.
[English, J. M.; Mills, M. J.; Bardeen, C. G.] Natl Ctr Atmospher Res, Earth Syst Lab, Boulder, CO 80307 USA.
[Thayer, J. P.] Univ Colorado, Dept Aerosp Engn Sci, Boulder, CO 80309 USA.
RP Neely, RR (reprint author), Univ Colorado, Dept Atmospher & Ocean Sci, Boulder, CO 80309 USA.
EM Ryan.Neely@colorado.edu
RI Neely, Ryan/F-8702-2010; Daniel, John/D-9324-2011; Mills,
Michael/B-5068-2010; Rosenlof, Karen/B-5652-2008; English,
Jason/E-9365-2015; THAYER, JEFFREY P./B-7264-2016; Manager, CSD
Publications/B-2789-2015
OI Neely, Ryan/0000-0003-4560-4812; Mills, Michael/0000-0002-8054-1346;
Rosenlof, Karen/0000-0002-0903-8270; English, Jason/0000-0001-9700-6860;
THAYER, JEFFREY P./0000-0001-7127-8251;
FU NOAA/ESRL-CIRES Graduate Fellowship program; NASA [NNX09AK71G]; NSF
[AGS-1135446, ATM-0856007]; National Science Foundation [CNS-0821794];
University of Colorado Boulder
FX The modeling was completed and analyzed by R. R. Neely during his PhD
funded through the NOAA/ESRL-CIRES Graduate Fellowship program. The work
represented by this paper was also supported by NASA Award NNX09AK71G
and NSF grant ATM-0856007. J. P. Thayer was supported by NSF grant
AGS-1135446. The modeling was completed and analyzed by R. R. Neely
during his PhD and funded through the NOAA/ESRL-CIRES Graduate
Fellowship program. The work represented by this paper was also
supported by NASA Award NNX09AK71G and NSF grant ATM-0856007. J. P.
Thayer was supported by NSF grant AGS-1135446. This work utilized the
Janus supercomputer, which is supported by the National Science
Foundation (award number CNS-0821794) and the University of Colorado
Boulder. The Janus supercomputer is a joint effort of the University of
Colorado Boulder, the University of Colorado Denver, and the National
Center for Atmospheric Research (NCAR). The NCAR is sponsored by the
National Science Foundation. The authors acknowledge the vision and
direction of the late D. Hofmann, which directly led to the experiment
and result discussed in this work. The authors also gratefully
acknowledge the helpful discussions from J. E. Barnes, D. M. Murphy, R.
Michael Hardesty, and Cora Randall. NCAR is sponsored by the National
Science Foundation. The authors acknowledge the vision and direction of
the late D. Hofmann, which directly led to the experiment and result
discussed in this work. The authors also gratefully acknowledge the
helpful discussions from J. E. Barnes, D. M. Murphy, R. Michael Hardesty
and Cora Randall.
NR 29
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U1 5
U2 54
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0094-8276
J9 GEOPHYS RES LETT
JI Geophys. Res. Lett.
PD MAR 16
PY 2013
VL 40
IS 5
BP 999
EP 1004
DI 10.1002/grl.50263
PG 6
WC Geosciences, Multidisciplinary
SC Geology
GA 134VG
UT WOS:000318242900037
ER
PT J
AU Gong, J
Wu, DL
AF Gong, Jie
Wu, Dong L.
TI View-angle-dependent AIRS cloudiness and radiance variance: Analysis and
interpretation
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
ID MOMENTUM TRANSPORT; INFRARED WINDOW; DIURNAL CYCLE; CONVECTION;
PRECIPITATION; ABSORPTION; RADIATION; CLOUDS; RADAR
AB Upper tropospheric clouds play an important role in the global energy budget and hydrological cycle. Significant view-angle asymmetry has been observed in upper-level tropical clouds derived from 8 years of Atmospheric Infrared Sounder (AIRS) 15 mm radiances. Here we find that the asymmetry also exists in the extratropics. It is larger during day than that during night, more prominent near elevated terrain, and closely associated with deep convection and wind shear. The cloud radiance variance, a proxy for cloud inhomogeneity, has consistent characteristics of the asymmetry to those in the AIRS cloudiness. The leading causes of the view-dependent cloudiness asymmetry are the local time difference and small-scale organized cloud structures. The local time difference (1-1.5 h) of upper-level clouds between two AIRS outermost views can create parts of the observed asymmetry. On the other hand, small-scale tilted and banded structures of the upper-level clouds can induce about half of the observed view-angle-dependent differences in the AIRS cloud radiances and their variances. This estimate is inferred from analogous study using microwave humidity sounder radiances observed during the period of time when there were simultaneous measurements at two different view-angles from NOAA-18 and NOAA-19 satellites. The existence of tilted cloud structures and asymmetric 15 mm and 6.7 mm cloud radiances implies that cloud statistics would be view-angle-dependent, and should be taken into account in radiative transfer calculations, measurement uncertainty evaluations and cloud climatology investigations. In addition, the momentum forcing in the upper troposphere from tilted clouds is also likely asymmetric, which can affect atmospheric circulation anisotropically.
C1 [Gong, Jie] NASA, Goddard Space Flight Ctr, Univ Space Res Assoc, Greenbelt, MD 20771 USA.
[Wu, Dong L.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Gong, J (reprint author), NASA, Goddard Space Flight Ctr, Univ Space Res Assoc, Greenbelt, MD 20771 USA.
EM Jie.gong@nasa.gov
FU NASA [NNH10ZDA001N]
FX This work is partly performed at Jet Propulsion Laboratory, and partly
at Goddard Space Flight Center with support from NASA
NNH10ZDA001N-ESDRERR (Earth System Data Records Uncertainty Analysis)
project. We are grateful for Dr. R. Vincent authorizing us to use his
radar image. Helpful discussions with B. Tian, Q. Yue, B. Khan, L. Chen,
J. Susskind, F. Zhang andmany other scientists are highly appreciated.
We thank two anonymous reviewers' comments and suggestions.
NR 44
TC 3
Z9 3
U1 0
U2 9
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-897X
EI 2169-8996
J9 J GEOPHYS RES-ATMOS
JI J. Geophys. Res.-Atmos.
PD MAR 16
PY 2013
VL 118
IS 5
BP 2327
EP 2339
DI 10.1002/jgrd.50120
PG 13
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 129LY
UT WOS:000317842800020
ER
PT J
AU Morishima, R
Golabek, GJ
Samuel, H
AF Morishima, Ryuji
Golabek, Gregor J.
Samuel, Henri
TI N-body simulations of oligarchic growth of Mars: Implications for Hf-W
chronology
SO EARTH AND PLANETARY SCIENCE LETTERS
LA English
DT Article
DE Mars; impacts; Hf-W chronometer; N-body simulations
ID MARTIAN HEMISPHERIC DICHOTOMY; CORE FORMATION; TERRESTRIAL PLANETS;
GIANT IMPACTS; MAGMA OCEAN; RUNAWAY GROWTH; RAPID GROWTH; ACCRETION;
PLANETESIMALS; DIFFERENTIATION
AB Dauphas and Pourmand [2011. Hf-W-Th evidence for rapid growth of Mars and its status as a planetary embryo. Nature 473, 489-492] estimated the accretion timescale of Mars to be 1.8(-1.0)(+0.9) Myr from the W isotopes of Martian meteorites. This timescale was derived assuming perfect metal-silicate equilibration between the impactor and the target's mantle. However, in the case of a small impactor most likely only a fraction of the target's mantle is involved in the equilibration, while only a small part of the impactor's core equilibrates in the case of a giant impact. We examined the effects of imperfect equilibration using results of high-resolution N-body simulations for the oligarchic growth stage. These effects were found to be small as long as a planetary embryo has a deep liquid magma ocean during its accretion. The effect due to partial involvement of the target's mantle in equilibration is small due to the low metal-silicate partition coefficient for W suggested from the low Hf/W ratio of the Martian mantle. The effect due to partial involvement of the impactor's core is also small because a large fraction of the embryo mass is delivered from small planetesimals, which are likely to fully equilibrate in the deep magma ocean on the embryo. The accretion timescale of Mars estimated by the Hf-W chronology is shorter than that expected for the minimum mass solar nebula model as long as more than 10% of each impactor's core re-equilibrates with the Martian mantle and the final stages of accretion are prolonged. This probably indicates that accretion of Mars rapidly proceeded due to solid and gas surface densities significantly larger than those for the minimum mass solar nebula or due to accretion of small fragments or pebbles. (C) 2013 Elsevier B.V. All rights reserved.
C1 [Morishima, Ryuji] Univ Calif Los Angeles, Inst Geophys & Planetary Phys, Los Angeles, CA 90095 USA.
[Morishima, Ryuji] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Golabek, Gregor J.] ENS Lyon, Lab Geol Lyon, F-69364 Lyon, France.
[Golabek, Gregor J.] Swiss Fed Inst Technol, Inst Geophys, CH-8092 Zurich, Switzerland.
[Samuel, Henri] Univ Bayreuth, Bayer Geoinst, D-95447 Bayreuth, Germany.
[Samuel, Henri] CNRS, Inst Rech Astrophys & Planetol, F-31400 Toulouse, France.
RP Morishima, R (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM Ryuji.Morishima@jpl.nasa.gov
FU NASA; SNF [PBEZP2-134461]; Stifterverband fur Deutsche Wissenschaft
FX We thank an anonymous reviewer and Alessandro Morbidelli for their
constructive comments and Hiroshi Kobayashi for fruitful discussions and
sending his preprint. This research was partly carried out at the Jet
Propulsion Laboratory, California Institute of Technology, under
contract with NASA. Government sponsorship is acknowledged. G.J.G. was
supported by SNF Grant PBEZP2-134461. H.S. acknowledges the funds from
the Stifterverband fur Deutsche Wissenschaft. The N-body simulations
were carried out on supercomputer Schrodinger at University of Zurich.
NR 59
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PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0012-821X
J9 EARTH PLANET SC LETT
JI Earth Planet. Sci. Lett.
PD MAR 15
PY 2013
VL 366
BP 6
EP 16
DI 10.1016/j.eps1.2013.01.036
PG 11
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 147OO
UT WOS:000319177100002
ER
PT J
AU Yokoyama, T
Misawa, K
Okano, O
Shih, CY
Nyquist, LE
Simon, JI
Tappa, MJ
Yoneda, S
AF Yokoyama, Tatsunori
Misawa, Keiji
Okano, Osamu
Shih, Chi-Yu
Nyquist, Laurence E.
Simon, Justin I.
Tappa, Michael J.
Yoneda, Shigekazu
TI Rb-Sr isotopic systematics of alkali-rich fragments in the Yamato-74442
LL-chondritic breccia
SO EARTH AND PLANETARY SCIENCE LETTERS
LA English
DT Article
DE chondritic breccias; moderately volatile elements; nebular condensation;
Rb-Sr dating
ID SOLAR NEBULA; IRON METEORITE; PARENT BODY; FRACTIONATION; CONDENSATION;
AGE; COSMOCHEMISTRY; CONSTRAINTS; CHRONOLOGY; CHONDRULES
AB We have undertaken mineralogical, petrographical and Rb-Sr isotopic studies on alkali-rich igneous rock fragments in the Yamato (Y)-74442 LL-chondritic breccia. The fragments are a few mm in size and are composed mainly of porphyritic olivine and dendritic pyroxene set in alkali-rich groundmass glass. Minor phases include chromite, troilite and metallic nickel-iron. Bulk chemical compositions of the fragments are almost identical to the host chondrite except for a depletion of sodium and an enrichment of potassium. Isotopic analyses of nine fragments from Y-74442 yield a Rb-Sr age of 4429 +/- 54 Ma (2 sigma) for 2(Rb-87)=0.01402 Ga-1 with an initial ratio of Sr-87/Sr-86 = 0.7144 +/- 0.0094 (2 sigma). Assuming precursors of the fragments formed 4568 Ma with 87Sr/86Sr= 0.69889 when the Solar System formed, a time-averaged Rb/Sr (weight) ratio of the source material for the fragments is calculated to be 2.58 +/- 0.91/0.93.
The extremely high Rb/Sr value of this source is difficult to interpret by any igneous fractionation or liquid immiscibility, but can be explained by mixing of a chondritic component with an alkali-rich component formed in the early solar nebula. In our preferred model, the alkali component with Rb/Sr >> 30 would have condensed from the residual nebular gas after removal of refractory strontium and must have been isolated for a long time in a region where the temperature was sufficiently low to prevent reaction with other silicates/oxides. A mixture of the alkali component (early nebular condensates) and the ferromagnesian component could reflect flash heating induced by impact on an LL-chondritic parent body at least 4429 Ma ago, and further enrichments of rubidium and potassium relative to strontium could have occurred during this event. The resulting impact-melt rocks could have been fragmented by later impact event(s) and finally incorporated into the Y-74442 parent body. Thus, a remarkable signature of alkali enrichments both in the early solar nebula and later on the LL-chondrite parent body is preserved as a minor component of some chondritic breccias such as Y-74442. (C) 2013 Elsevier B.V. All rights reserved.
C1 [Yokoyama, Tatsunori; Misawa, Keiji] Grad Univ Adv Studies SOKENDAI, Dept Polar Sci, Tachikawa, Tokyo 1908518, Japan.
[Yokoyama, Tatsunori; Misawa, Keiji] Lunar & Planetary Inst, Univ Space Res Assoc, Houston, TX 77058 USA.
[Misawa, Keiji] Natl Inst Polar Res, Tachikawa, Tokyo 1908518, Japan.
[Okano, Osamu] Okayama Univ, Grad Sch Nat Sci & Technol, Okayama 7008530, Japan.
[Shih, Chi-Yu; Tappa, Michael J.] ESCG Jacobs Technol, Houston, TX 77258 USA.
[Nyquist, Laurence E.; Simon, Justin I.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA.
[Yoneda, Shigekazu] Natl Museum Nat & Sci, Tsukuba, Ibaraki 3050005, Japan.
RP Misawa, K (reprint author), Natl Inst Polar Res, 10-3 Midoricho, Tachikawa, Tokyo 1908518, Japan.
EM misawa@nipr.ac.jp
FU NIPR Research Program [KP-6]; Graduate University for Advanced Studies
(SOKENDAI); Lunar and Planetary Institute (LPI); NASA [10-LASER10-0077]
FX We are grateful to the National Institute of Polar Research and the
Smithsonian National Museum of Natural History for allocating the
meteorite specimens of Yamato-74442 and Bhola (USNM 1806), respectively.
Two polished thin sections, Krahenberg (section A) and Bhola (MPK3042L),
were loaned from the Senkenberg Forschungsinstitut und Naturmuseum
Frankfurt. TY is grateful to the staff of SEM-EPMA Laboratory at NIPR
for their help during the course of analysis. He wants to thank H.
Minowa and T. Fukuoka for their help and suggestion during the course of
IP experiments. Constructive comments from H. Palme and an anonymous
reviewer improved and clarified the manuscript. Furthermore, we would
like to thank B. Marty for editorial handling of the manuscript. This
work was partly supported by funds from the NIPR Research Program
(KP-6), The Graduate University for Advanced Studies (SOKENDAI), Lunar
and Planetary Institute (LPI) and NASA (10-LASER10-0077 to JIS). This is
LPI contribution 1717.
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PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0012-821X
J9 EARTH PLANET SC LETT
JI Earth Planet. Sci. Lett.
PD MAR 15
PY 2013
VL 366
BP 38
EP 48
DI 10.1016/j.epsl.2013.01.037
PG 11
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 147OO
UT WOS:000319177100005
ER
PT J
AU Ruane, AC
Cecil, LD
Horton, RM
Gordon, R
McCollum, R
Brown, D
Killough, B
Goldberg, R
Greeley, AP
Rosenzweig, C
AF Ruane, Alex C.
Cecil, L. DeWayne
Horton, Radley M.
Gordon, Roman
McCollum, Raymond
Brown, Douglas
Killough, Brian
Goldberg, Richard
Greeley, Adam P.
Rosenzweig, Cynthia
TI Climate change impact uncertainties for maize in Panama: Farm
information, climate projections, and yield sensitivities
SO AGRICULTURAL AND FOREST METEOROLOGY
LA English
DT Article
DE Climate change; Crop modeling; Uncertainty; Adaptation; Panama; Maize;
GCM ensembles
ID ELEVATED CO2; CROP YIELD; MODEL; FOOD; STIMULATION; RISK
AB We present results from a pilot project to characterize and bound multi-disciplinary uncertainties around the assessment of maize (Zea mays) production impacts using the CERES-Maize crop model in a climate-sensitive region with a variety of farming systems (Panama). Segunda coa (autumn) maize yield in Panama currently suffers occasionally from high water stress at the end of the growing season, however under future climate conditions warmer temperatures accelerate crop maturation and elevated CO2 concentrations improve water retention. This combination reduces end-of-season water stresses and eventually leads to small mean yield gains according to median projections, although accelerated maturation reduces yields in seasons with low water stresses. Calibrations of cultivar traits, soil profile, and fertilizer amounts are most important for representing baseline yields, however sensitivity to all management factors are reduced in an assessment of future yield changes (most dramatically for fertilizers), suggesting that yield changes may be more generalizable than absolute yields. Uncertainty around GCMs' projected changes in rainfall gain in importance throughout the century, with yield changes strongly correlated with growing season rainfall totals. Climate changes are expected to be obscured by the large interannual variations in Panamanian climate that will continue to be the dominant influence on seasonal maize yield into the coming decades. The relatively high (A2) and low (B1) emissions scenarios show little difference in their impact on future maize yields until the end of the century. Uncertainties related to the sensitivity of CERES-Maize to carbon dioxide concentrations have a substantial influence on projected changes, and remain a significant obstacle to climate change impacts assessment. Finally, an investigation into the potential of simple statistical yield emulators based upon key climate variables characterizes the important uncertainties behind the selection of climate change metrics and their performance against more complex process-based crop model simulations, revealing a danger in relying only on long-term mean quantities for crop impact assessment. Published by Elsevier B.V.
C1 [Ruane, Alex C.; Horton, Radley M.; Rosenzweig, Cynthia] NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
[Ruane, Alex C.; Horton, Radley M.; Goldberg, Richard; Greeley, Adam P.; Rosenzweig, Cynthia] Columbia Univ, Ctr Climate Syst Res, New York, NY USA.
[Cecil, L. DeWayne] NOAA, Natl Climat Data Ctr, Salt Lake City, UT USA.
[Gordon, Roman] Inst Invest Agr Panama, Los Santos, Panama.
[McCollum, Raymond; Brown, Douglas] Booze Allen Hamilton, Norfolk, VA USA.
[Killough, Brian] NASA, Langley Res Ctr, Langley, VA USA.
RP Ruane, AC (reprint author), 2880 Broadway, New York, NY 10025 USA.
EM alexander.c.ruane@nasa.gov
FU NASA [NNX10AO10G]
FX The views expressed in this article are those of the authors, and do not
necessarily represent those of the authors' institutions. This project
was initiated by L. DeWayne Cecil when he was serving in the capacity of
Senior Science Advisor to the NASA Langley Systems Engineering Office
for the international Committee on Earth Observing Satellites (CEOS).
Development of this study was also partially supported by NASA
NNX10AO10G. We acknowledge the modeling groups, the Program for Climate
Model Diagnosis and Intercomparison (PCMDI) and the WCRP Working Group
on Coupled Modeling (WGCM) for their roles in making available the WCRP
CMIP3 multi-model dataset. Support of this dataset is provided by the
Office of Science, U.S. Department of Energy. We are grateful to Berta
Olmedo and ETESA for providing Los Santos weather data, Ismael Camargo
for helping to track down maize field trial data, and those who took
weather and field observations. We also acknowledge the editor and two
reviewers for helping to spur a more robust study made possible through
the collection of additional data and model updates.
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PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0168-1923
EI 1873-2240
J9 AGR FOREST METEOROL
JI Agric. For. Meteorol.
PD MAR 15
PY 2013
VL 170
SI SI
BP 132
EP 145
DI 10.1016/j.agrformet.2011.10.015
PG 14
WC Agronomy; Forestry; Meteorology & Atmospheric Sciences
SC Agriculture; Forestry; Meteorology & Atmospheric Sciences
GA 098JX
UT WOS:000315546700013
ER
PT J
AU Rosenzweig, C
Jones, JW
Hatfield, JL
Ruane, AC
Boote, KJ
Thorburn, P
Antle, JM
Nelson, GC
Porter, C
Janssen, S
Asseng, S
Basso, B
Ewert, F
Wallach, D
Baigorria, G
Winter, JM
AF Rosenzweig, C.
Jones, J. W.
Hatfield, J. L.
Ruane, A. C.
Boote, K. J.
Thorburn, P.
Antle, J. M.
Nelson, G. C.
Porter, C.
Janssen, S.
Asseng, S.
Basso, B.
Ewert, F.
Wallach, D.
Baigorria, G.
Winter, J. M.
TI The Agricultural Model Intercomparison and Improvement Project (AgMIP):
Protocols and pilot studies
SO AGRICULTURAL AND FOREST METEOROLOGY
LA English
DT Article
DE Agriculture; Food security; Climate change; Crop models; Economic
models; Intercomparison; Uncertainty; Risk; Adaptation
ID STOCHASTIC WEATHER GENERATORS; CLIMATE-CHANGE RESEARCH; CROPGRO-SOYBEAN
MODEL; INTEGRATED ASSESSMENT; US AGRICULTURE; SYSTEM MODEL; ELEVATED
CO2; YIELD; IMPACTS; VARIABILITY
AB The Agricultural Model Intercomparison and Improvement Project (AgMIP) is a major international effort linking the climate, crop, and economic modeling communities with cutting-edge information technology to produce improved crop and economic models and the next generation of climate impact projections for the agricultural sector. The goals of AgMIP are to improve substantially the characterization of world food security due to climate change and to enhance adaptation capacity in both developing and developed countries. Analyses of the agricultural impacts of climate variability and change require a transdisciplinary effort to consistently link state-of-the-art climate scenarios to crop and economic models. Crop model outputs are aggregated as inputs to regional and global economic models to determine regional vulnerabilities, changes in comparative advantage, price effects, and potential adaptation strategies in the agricultural sector. Climate, Crop Modeling, Economics, and Information Technology Team Protocols are presented to guide coordinated climate, crop modeling, economics, and information technology research activities around the world, along with AgMIP Cross-Cutting Themes that address uncertainty, aggregation and scaling, and the development of Representative Agricultural Pathways (RAPs) to enable testing of climate change adaptations in the context of other regional and global trends. The organization of research activities by geographic region and specific crops is described, along with project milestones.
Pilot results demonstrate AgMIP's role in assessing climate impacts with explicit representation of uncertainties in climate scenarios and simulations using crop and economic models. An intercomparison of wheat model simulations near Obregon, Mexico reveals inter-model differences in yield sensitivity to [CO2] with model uncertainty holding approximately steady as concentrations rise, while uncertainty related to choice of crop model increases with rising temperatures. Wheat model simulations with mid-century climate scenarios project a slight decline in absolute yields that is more sensitive to selection of crop model than to global climate model, emissions scenario, or climate scenario downscaling method. A comparison of regional and national-scale economic simulations finds a large sensitivity of projected yield changes to the simulations' resolved scales. Finally, a global economic model intercomparison example demonstrates that improvements in the understanding of agriculture futures arise from integration of the range of uncertainty in crop, climate, and economic modeling results in multi-model assessments. (C) 2012 Published by Elsevier B.V.
C1 [Rosenzweig, C.; Ruane, A. C.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
[Rosenzweig, C.; Ruane, A. C.; Winter, J. M.] Columbia Univ, Ctr Climate Syst Res, New York, NY USA.
[Jones, J. W.; Boote, K. J.; Porter, C.; Asseng, S.] Univ Florida, Gainesville, FL USA.
[Hatfield, J. L.] ARS, Natl Lab Agr & Environm, USDA, Ames, IA USA.
[Thorburn, P.] Commonwealth Sci & Ind Res Org, Brisbane, Qld, Australia.
[Antle, J. M.] Oregon State Univ, Corvallis, WA USA.
[Nelson, G. C.] Int Food Policy Res Inst, Washington, DC 20036 USA.
[Janssen, S.] Wageningen Univ & Res Ctr, Alterra, Wageningen, Netherlands.
[Basso, B.] Michigan State Univ, E Lansing, MI 48824 USA.
[Ewert, F.] Univ Bonn, Bonn, Germany.
[Wallach, D.] INRA, F-31931 Toulouse, France.
[Baigorria, G.] Univ Nebraska Lincoln, Lincoln, NE USA.
RP Rosenzweig, C (reprint author), NASA, Goddard Inst Space Studies, 2880 Broadway, New York, NY 10025 USA.
EM cynthia.rosenzweig@nasa.gov
RI Basso, Bruno/A-3128-2012; Thorburn, Peter/A-6884-2011;
OI Basso, Bruno/0000-0003-2090-4616; Boote, Kenneth/0000-0002-1358-5496;
Wallach, Daniel/0000-0003-3500-8179
FU United States Department of Agriculture; UK Department for International
Development
FX We acknowledge the significant contribution to the development of AgMIP
by our esteemed colleague, the late Dr. Nadine Brisson of L'Institut
National de la Recherche Agronomique. We are grateful to all of our
colleagues from the international agricultural research community who
have helped to create AgMIP since its inception at the University of
Florida Climate Information for Managing Risks Conference in 2008, and
those who are participating in current AgMIP activities. We appreciate
especially the expert advice provided by the AgMIP Steering Group. We
thank Carlos Angulo from University of Bonn for providing assistance
with crop simulations, and Richard Goldberg, Adam Greeley, Daniel Bader,
and Soyee Chiu at the Columbia Center for Climate Systems Research for
their help in processing climate and data. We acknowledge the global
climate modeling groups, the Program for Climate Model Diagnosis and
Intercomparison (PCMDI), and the WCRP's Working Group on Coupled
Modelling (WGCM) for their roles in making available the WCRP CMIP3
multi-model dataset. Support of this dataset is provided by the Office
of Science, U.S. Department of Energy. We appreciate the constructive
suggestions of three anonymous reviewers. Finally, we thank the United
States Department of Agriculture and the UK Department for International
Development for their support of AgMIP, and in particular Steven Shafer
and William Hohenstein at USDA, and Alessandro Moscuzza, Gemma Tanner,
Robert MacIver, and Yvan Blot at UK DFID for their guidance.
NR 113
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PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0168-1923
EI 1873-2240
J9 AGR FOREST METEOROL
JI Agric. For. Meteorol.
PD MAR 15
PY 2013
VL 170
SI SI
BP 166
EP 182
DI 10.1016/j.agrformet.2012.09.011
PG 17
WC Agronomy; Forestry; Meteorology & Atmospheric Sciences
SC Agriculture; Forestry; Meteorology & Atmospheric Sciences
GA 098JX
UT WOS:000315546700015
ER
PT J
AU Zhang, FF
Yan, C
Teng, HH
Roden, EE
Xu, HF
AF Zhang, Fangfu
Yan, Chao
Teng, H. Henry
Roden, Eric E.
Xu, Huifang
TI In situ AFM observations of Ca-Mg carbonate crystallization catalyzed by
dissolved sulfide: Implications for sedimentary dolomite formation
SO GEOCHIMICA ET COSMOCHIMICA ACTA
LA English
DT Article
ID ATOMIC-FORCE MICROSCOPY; SULFATE-REDUCING BACTERIA; CALCITE GROWTH;
DISSOLUTION KINETICS; DISORDERED DOLOMITE; AQUEOUS-SOLUTION; ORGANOGENIC
DOLOMITIZATION; MICROBIAL MEDIATION; SURFACE PROCESSES; SEA-WATER
AB It has been observed that the metabolism of sulfate-reducing bacteria can overcome the energy barrier to Mg2+ incorporation into growing Ca-Mg carbonates and enhance dolomite precipitation, although the role of SRB in dolomite formation is still under debate. In this study, we presented in situ AFM observations of Ca-Mg carbonate {104} surface growing from supersaturated solutions. Our data showed that not only can Mg2+ modify the morphology of the polygonal growth hillocks and impede step growth, but it can also inhibit 1-D step nucleation, resulting in the inability for spirals to continue their vertical growth. However, in the presence of dissolved sulfide, both the 1-D step nucleation and step growth which had been retarded by Mg2+ ions were significantly enhanced. For example, in the presence as low as 0.13 mM dissolved sulfide, the step velocity can be increased by more than 9 times compared to that in contact with solutions containing Mg2+ ions but no dissolved sulfide. The Ca-Mg carbonate growth hillock in contact with dissolved sulfide-bearing growth solutions eventually developed a micromosaic-like structure. Based on our observations, we propose that the overall catalytic effect of dissolved sulfide may be twofold, one to stabilize the critical nuclei during 1-D step nucleation by the adsorption of dissolved sulfide on Ca-Mg carbonate surfaces and two to facilitate the dehydration of surface Mg2+-water complexes during growth. We hypothesize that dissolved sulfide may adsorb on crystal faces through hydrogen bonding between the H in HS-/H2S and the O in calcite CO32- to weaken the rigid Mg2+ hydration shell, resulting in an elevated activation entropy for particle attachment and hence a larger kinetic coefficient for step growth. Together with previous studies on disorder dolomite precipitation induced by dissolved sulfide, we demonstrate the catalysis role of dissolved sulfide in sedimentary dolomite formation associate with SRB, which may shed new light on the long-standing "dolomite problem". (C) 2012 Elsevier Ltd. All rights reserved.
C1 [Zhang, Fangfu; Roden, Eric E.; Xu, Huifang] Univ Wisconsin, Dept Geosci, NASA Astrobiol Inst, Madison, WI 53706 USA.
[Yan, Chao; Teng, H. Henry] George Washington Univ, Dept Chem, Washington, DC 20052 USA.
RP Xu, HF (reprint author), Univ Wisconsin, Dept Geosci, NASA Astrobiol Inst, 1215 W Dayton St, Madison, WI 53706 USA.
EM hfxu@geology.wisc.edu
RI Zhang, Fangfu/B-4295-2014
OI Zhang, Fangfu/0000-0001-7550-9483
FU NASA Astrobiology Institute [N07-5489]; NSF [EAR-095800]; U.S.
Department of Energy [DE-SC0001929]; Department of Geoscience,
University of Wisconsin-Madison; Geological Society of America
FX This work was supported by NASA Astrobiology Institute (N07-5489), NSF
(EAR-095800), and U.S. Department of Energy (DE-SC0001929). Zhang thanks
Department of Geoscience, University of Wisconsin-Madison and ExxonMobil
for 2008 Summer Research Grant, and Geological Society of America for
2009 Graduate Research Grant. We thank Prof. Liane Benning for handling
this paper and the three anonymous reviewers for their comments and
suggestions which greatly improved this paper.
NR 76
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PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0016-7037
J9 GEOCHIM COSMOCHIM AC
JI Geochim. Cosmochim. Acta
PD MAR 15
PY 2013
VL 105
BP 44
EP 55
DI 10.1016/j.gca.2012.11.010
PG 12
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 093MA
UT WOS:000315194800004
ER
PT J
AU Cartwright, JA
Ott, U
Mittlefehldt, DW
Herrin, JS
Herrmann, S
Mertzman, SA
Mertzman, KR
Peng, ZX
Quinn, JE
AF Cartwright, J. A.
Ott, U.
Mittlefehldt, D. W.
Herrin, J. S.
Herrmann, S.
Mertzman, S. A.
Mertzman, K. R.
Peng, Z. X.
Quinn, J. E.
TI The quest for regolithic howardites. Part 1: Two trends uncovered using
noble gases
SO GEOCHIMICA ET COSMOCHIMICA ACTA
LA English
DT Article
ID ASTEROID 4 VESTA; CARBONACEOUS CHONDRITE CLASTS; ARGON ISOTOPIC
VARIATIONS; CALCIUM-RICH ACHONDRITES; ANCIENT SOLAR-ACTIVITY; DIOGENITE
PARENT BODY; RAY EXPOSURE AGES; ANGRA-DOS-REIS; BASALTIC ACHONDRITES;
ANTARCTIC METEORITES
AB We report noble gas data (helium (He), neon (Ne), argon (Ar), krypton (Kr) and xenon (Xe)), nominal gas retention ages (K-Ar, U-Th-He) and cosmic ray exposure (CRE) ages for the ten howardites EET 83376, EET 99408, LEW 85313, MET 00423, MET 96500, PCA 02066, PRA 04401, QUE 94200, QUE 97002, and SCO 06040, in research to better understand the regolith of the HED parent body - Vesta - through a combined petrological, compositional and noble gas study. Our main aim is to determine which howardites are truly regolithic - as defined by the presence of solar noble gas components (e.g. solar wind (SW), fractionated solar wind (FSW)) and/or by the presence of planetary components (e.g. Q, HL) associated with foreign clasts of carbonaceous chondrite material within the breccias.
Of our ten howardites, four (LEW 85313, MET 00423, PRA 04401 and SCO 06040) show evidence for a regolithic origin, with noble gas ratios indicating the presence of trapped components. Howardites PRA 04401 and SCO 06040 contain significant amounts of CM type carbonaceous chondrite material, and these samples are dominated by a planetary component similar to that observed in CM meteorites Murchison and Maribo. Overall, we find evidence for two regolithic groups with different release trends: (1) SW/FSW component dominated howardites (LEW 85313 and MET 00423), where SW/FSW is dominant at low temperature releases, and less pronounced at higher temperatures; (2) Planetary component dominated howardites (PRA 04401 and SCO 06040) that also contain SW/FSW - the planetary component is associated with incorporated carbonaceous chondrite material, and is dominant at the mid-temperature release. The remaining six howardites EET 83376, EET 99408, MET 96500, PCA 02066, QUE 94200, and QUE 97002, are dominated by cosmogenic noble gases, and are not considered regolithic.
Previous work by Warren et al. (2009) suggested that high siderophile element contents (specifically nickel (Ni) > 300 mu g/g) were a regolith indicator for howardites, in addition to restricted Al2O3 contents (8-9 wt.%) representing a eucrite/diogenite mixing ratio of 2: 1 as indicative of an ancient well-mixed regolith. These parameters were based on five 'gas-rich' howardites. However, we find no obvious correlation between these parameters and SW/FSW or planetary noble gas content in our howardite samples. We conclude that howardite regolith parameters are not as simple as those defined by Warren et al. (2009), where three of the five howardites used contained foreign CM material, which may have caused a bias in their defined parameters. We conclude that sideophile abundances alone cannot be used to determine the regolithic nature of a sample: noble gas analysis remains a key parameter, where it is important to distinguish between planetary-dominated and SW-dominated regolithic howardites. (C) 2012 Elsevier Ltd. All rights reserved.
C1 [Cartwright, J. A.; Ott, U.; Herrmann, S.] Max Planck Inst Chem, D-55128 Mainz, Germany.
[Ott, U.] Univ Western Hungary, H-9700 Szombathely, Hungary.
[Mittlefehldt, D. W.] NASA, Lyndon B Johnson Space Ctr, Astromat Res Off, Houston, TX 77058 USA.
[Herrin, J. S.; Peng, Z. X.; Quinn, J. E.] Engn & Sci Contract Grp, Houston, TX 77258 USA.
[Mertzman, S. A.; Mertzman, K. R.] Franklin & Marshall Coll, Dept Earth & Environm, Lancaster, PA 17604 USA.
RP Cartwright, JA (reprint author), CALTECH, Div Geol & Planetary Sci, MC 100-23,1200 E Calif Blvd, Pasadena, CA 91125 USA.
EM jac@caltech.edu
RI Cartwright, Julia/A-8470-2013;
OI Herrin, Jason/0000-0002-2452-244X
FU National Science Foundation; NASA's Cosmochemistry Program
FX We thank the National Science Foundation for funding the ANSMET
collecting teams that brought back the Antarctic samples studied here,
and the Meteorite Working Group, NASA-Johnson Space Center and the
National Museum of Natural History (Smithsonian Institution) for
allocation of the samples. We are grateful to K. McBride and C.
Satterwhite for extraction of the samples used in this work. DWM's
participation in this project, and bulk sample major and trace element
analyses were funded through NASA's Cosmochemistry Program. We would
also like to thank two anonymous reviewers and the associate editor
Anders Meilbom, who's comments and contributions aided the manuscript.
NR 124
TC 14
Z9 14
U1 1
U2 19
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0016-7037
J9 GEOCHIM COSMOCHIM AC
JI Geochim. Cosmochim. Acta
PD MAR 15
PY 2013
VL 105
BP 395
EP 421
DI 10.1016/j.gca.2012.11.047
PG 27
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 093MA
UT WOS:000315194800023
ER
PT J
AU Arnesen, AS
Silva, TSF
Hess, LL
Novo, EMLM
Rudorff, CM
Chapman, BD
McDonald, KC
AF Arnesen, Allan S.
Silva, Thiago S. F.
Hess, Laura L.
Novo, Evlyn M. L. M.
Rudorff, Conrado M.
Chapman, Bruce D.
McDonald, Kyle C.
TI Monitoring flood extent in the lower Amazon River floodplain using
ALOS/PALSAR ScanSAR images
SO REMOTE SENSING OF ENVIRONMENT
LA English
DT Article
DE Object-based image analysis; Multi-temporal analysis; Incidence angle;
Wetlands; Synthetic aperture radar; Kyoto & Carbon Initiative
ID METHANE EMISSIONS; SAR DATA; VEGETATION; RADAR; BASIN; WETLANDS;
INUNDATION; HYDROLOGY; MISSION; SCALE
AB The Amazon River floodplain is subject to large seasonal variations in water level and flood extent, due to the large size and low relief of the basin, and the large amount of precipitation in the region. Synthetic Aperture Radar (SAR) data can be used to map flooded area in these wetlands, given its ability to provide continuous information without being heavily affected by cloud cover. As part of JAXA's Kyoto & Carbon Initiative, extensive wide-swath, multi-temporal SAR coverage of the Amazon basin has been obtained using the ScanSAR mode of ALOS PALSAR This study presents a method for monitoring flood extent variation using ALOS ScanSAR images, tested at the Curuai Lake floodplain, in the lower Amazon River, Brazil. Twelve ScanSAR scenes were acquired between 2006 and 2010, including seven during the 2007 hydrological year. Water level records, field photographs, optical images (Landsat-5/TM and MODIS/Ferra and Aqua) and topographic data were used as auxiliary information. A data mining algorithm allowed the implementation of a hierarchical, object-based classification algorithm, able to map land cover types and flooding status in the study area for all available dates. land cover based on the entire time series (classification levels 1 and 2) had overall accuracies of 90% and 83%, respectively. Level 3 classifications (one map per image date) were validated only for the lowest and highest water stages, with overall accuracies of 76% and 78%, respectively. Total flood extent (Level 4) was mapped with 84% and 94% accuracies, for the low and high water stages, respectively. Regression models were fitted between mapped flooded area and water levels at the Curuai gauge to predict flood extent. A polynomial model had R-2=0.95 (p<0.05) and an overall root mean square error (RMSE) of 241 km(2), while a logistic model had R-2=0.98 (p<0.05) and RMSE = 127 km(2). (C) 2012 Elsevier Inc. All rights reserved.
C1 [Arnesen, Allan S.; Silva, Thiago S. F.; Novo, Evlyn M. L. M.] Inst Nacl Pesquisas Espaciais, Div Sensoriamento Remoto, BR-12201970 Sao Jose Dos Campos, Brazil.
[Hess, Laura L.] Univ Calif Santa Barbara, Earth Res Inst, Santa Barbara, CA 93106 USA.
[Rudorff, Conrado M.] Univ Calif Santa Barbara, Bren Sch Environm Sci & Management, Santa Barbara, CA 93106 USA.
[Chapman, Bruce D.; McDonald, Kyle C.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[McDonald, Kyle C.] CUNY City Coll, Dept Earth & Atmospher Sci, CUNY Environm Crossrd Initiat, New York, NY 10031 USA.
[McDonald, Kyle C.] CUNY City Coll, CUNY CREST Inst, New York, NY 10031 USA.
RP Arnesen, AS (reprint author), Inst Nacl Pesquisas Espaciais, Div Sensoriamento Remoto, Caixa Postal 515, BR-12201970 Sao Jose Dos Campos, Brazil.
EM allansarnesen@gmail.com
RI Silva, Thiago/A-2444-2009; Rudorff, Conrado/E-9851-2013; chen,
zhu/K-5923-2013; Ma, Lei/I-4597-2014
OI Silva, Thiago/0000-0001-8174-0489; Rudorff, Conrado/0000-0001-8453-1367;
FU Brazilian National Council for Scientific and Technological Development
(CNPq) [130519/2010-3]; Sao Paulo Research Foundation (FAPESP)
[2008/07537-1, 2010/11269-2]; Ministry of Education of Brazil through a
CAPES/Fulbright Award [1705-07-5]; NASA Making Earth Science Data
Records for Use in Research Environments (MEaSUREs) program [NNX11AQ39G]
FX The authors wish to acknowledge the Brazilian National Council for
Scientific and Technological Development (CNPq) for the fellowship
supporting Allan Amesen through his graduate program (130519/2010-3),
and the Sao Paulo Research Foundation (FAPESP) for the financial support
during the field campaign in April 2011 (2008/07537-1) and Dr. Silva's
post-doctoral grant (2010/11269-2). Conrado Rudorff was funded by the
Ministry of Education of Brazil through a CAPES/Fulbright Award
(1705-07-5). The authors also thank Dr. Claudio Barbosa for providing
bathymetry data from his extensive sonar surveys. This work has been
undertaken within the framework of JAXA's Kyoto & Carbon Initiative,
with ALOS PALSAR data provided by JAXA EORC, and supported by the NASA
Making Earth Science Data Records for Use in Research Environments
(MEaSUREs) program under grant number NNX11AQ39G. More information on
the MEaSUREs project may be found at http://wetlands.jpl.nasa.gov.
Portions of this work were carried out at the Jet Propulsion Laboratory,
California Institute of Technology under contract to the National
Aeronautics and Space Administration.
NR 43
TC 27
Z9 29
U1 4
U2 121
PU ELSEVIER SCIENCE INC
PI NEW YORK
PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA
SN 0034-4257
J9 REMOTE SENS ENVIRON
JI Remote Sens. Environ.
PD MAR 15
PY 2013
VL 130
BP 51
EP 61
DI 10.1016/j.rse.2012.10.035
PG 11
WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic
Technology
SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science &
Photographic Technology
GA 090VL
UT WOS:000315008000005
ER
PT J
AU Naesset, E
Gobakken, T
Bollandsas, OM
Gregoire, TG
Nelson, R
Stahl, G
AF Naesset, Erik
Gobakken, Terje
Bollandsas, Ole Martin
Gregoire, Timothy G.
Nelson, Ross
Stahl, Goran
TI Comparison of precision of biomass estimates in regional field sample
surveys and airborne LiDAR-assisted surveys in Hedmark County, Norway
SO REMOTE SENSING OF ENVIRONMENT
LA English
DT Article
DE Forest monitoring; Airborne LiDAR; Probability sampling; Biomass
estimation; Model-assisted estimation
ID LASER SCANNER DATA; FOREST BIOMASS; PLOT SIZE; INVENTORY; CARBON;
ICESAT/GLAS; INFERENCE; ACCURACY; VOLUME; AREA
AB Airborne scanning LiDAR (Light Detection and Ranging) has emerged as a promising tool to provide auxiliary data for sample surveys aiming at estimation of above-ground tree biomass (AGB), with potential applications in REDD forest monitoring. For larger geographical regions such as counties, states or nations, it is not feasible to collect airborne LiDAR data continuously ("wall-to-wall") over the entire area of interest. Two-stage cluster survey designs have therefore been demonstrated by which LiDAR data are collected along selected individual flight-lines treated as clusters and with ground plots sampled along these LiDAR swaths. Recently, analytical AGB estimators and associated variance estimators that quantify the sampling variability have been proposed. Empirical studies employing these estimators have shown a seemingly equal or even larger uncertainty of the AGB estimates obtained with extensive use of LiDAR data to support the estimation as compared to pure field-based estimates employing estimators appropriate under simple random sampling (SRS). However, comparison of uncertainty estimates under SRS and sophisticated two-stage designs is complicated by large differences in the designs and assumptions. In this study, probability-based principles to estimation and inference were followed. We assumed designs of a field sample and a LiDAR-assisted survey of Hedmark County (HC) (27,390 km(2)), Norway, considered to be more comparable than those assumed in previous studies. The field sample consisted of 659 systematically distributed National Forest Inventory (NFI) plots and the airborne scanning LiDAR data were collected along 53 parallel flight-lines flown over the NFI plots. We compared AGB estimates based on the field survey only assuming SRS against corresponding estimates assuming two-phase (double) sampling with LiDAR and employing model-assisted estimators. We also compared AGB estimates based on the field survey only assuming two-stage sampling (the NFI plots being grouped in clusters) against corresponding estimates assuming two-stage sampling with the LiDAR and employing model-assisted estimators. For each of the two comparisons, the standard errors of the AGB estimates were consistently lower for the LiDAR-assisted designs. The overall reduction of the standard errors in the LiDAR-assisted estimation was around 40-60% compared to the pure field survey. We conclude that the previously proposed two-stage model-assisted estimators are inappropriate for surveys with unequal lengths of the LiDAR flight-lines and new estimators are needed. Some options for design of LiDAR-assisted sample surveys under REDD are also discussed, which capitalize on the flexibility offered when the field survey is designed as an integrated part of the overall survey design as opposed to previous LiDAR-assisted sample surveys in the boreal and temperate zones which have been restricted by the current design of an existing NFT. (C) 2012 Elsevier Inc. All rights reserved.
C1 [Naesset, Erik; Gobakken, Terje; Bollandsas, Ole Martin] Norwegian Univ Life Sci, Dept Ecol & Nat Resource Management, NO-1432 As, Norway.
[Gregoire, Timothy G.] Yale Univ, Sch Forestry & Environm Studies, New Haven, CT 06511 USA.
[Nelson, Ross] NASA, Goddard Space Flight Ctr, Biospher Sci Branch, Greenbelt, MD 20771 USA.
[Stahl, Goran] Swedish Univ Agr Sci, Dept Forest Resource Management, SE-90183 Umea, Sweden.
RP Naesset, E (reprint author), Norwegian Univ Life Sci, Dept Ecol & Nat Resource Management, POB 5003, NO-1432 As, Norway.
EM erik.naesset@umb.no
RI Nelson, Ross/H-8266-2014
FU Research Council of Norway [166482/i10, 184636/S30]
FX This research has been funded by the Research Council of Norway (project
#166482/i10 and #184636/S30). The authors would like to thank the
Norwegian National Forest Inventory for collection of field data and
Blom Geomatics, Norway, for collection and processing of the airborne
LiDAR data.
NR 46
TC 37
Z9 39
U1 6
U2 89
PU ELSEVIER SCIENCE INC
PI NEW YORK
PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA
SN 0034-4257
J9 REMOTE SENS ENVIRON
JI Remote Sens. Environ.
PD MAR 15
PY 2013
VL 130
BP 108
EP 120
DI 10.1016/j.rse.2012.11.010
PG 13
WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic
Technology
SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science &
Photographic Technology
GA 090VL
UT WOS:000315008000010
ER
PT J
AU Ahmed, R
Siqueira, P
Hensley, S
AF Ahmed, Razi
Siqueira, Paul
Hensley, Scott
TI A study of forest biomass estimates from lidar in the northern temperate
forests of New England
SO REMOTE SENSING OF ENVIRONMENT
LA English
DT Article
DE Lidar; Forest biomass; Harvard Forest; Howland Forest
ID LARGE-FOOTPRINT LIDAR; PACIFIC-NORTHWEST; CANOPY STRUCTURE; STAND;
VEGETATION; EQUATIONS
AB Quantification of global carbon storage, carbon flux and disturbance in forested regions is of critical importance to refining our understanding of ecosystem processes, climate modeling and climate change. Remote sensing instruments, such as lidar and radar provide a means of obtaining highly accurate and well resolved biomass estimates over global scales. This has sparked interest in mission concepts such as DESDynI. One of the core objectives of the proposed DESDynI mission was global carbon accounting and monitoring through a combination of lidar and radar measurements. In this article, the relationship between field biomass and lidar metrics is analyzed using data from coordinated field measurements and lidar overflights at the Harvard and Howland Forests in North-Eastern United States to assess the performance of a potential biomass mapping instrument. Results show that the performance of lidar estimates of biomass vary significantly between the two sites even though they belong to the same northern temperate forest ecoregion. An attempt is made to isolate the reasons behind the dissimilarities. While RMS errors as low as 30 tons/ha can be seen, these are limited to biomass ranges of up to 300 tons/ha. (C) 2012 Elsevier Inc. All rights reserved.
C1 [Ahmed, Razi; Hensley, Scott] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Siqueira, Paul] Univ Massachusetts, Amherst, MA 01003 USA.
RP Ahmed, R (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA USA.
EM razi.u.ahmed@jpl.nasa.gov
RI Beckley, Matthew/D-4547-2013; Siqueira, Paul/D-9760-2016
OI Siqueira, Paul/0000-0001-5781-8282
NR 21
TC 11
Z9 12
U1 4
U2 74
PU ELSEVIER SCIENCE INC
PI NEW YORK
PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA
SN 0034-4257
J9 REMOTE SENS ENVIRON
JI Remote Sens. Environ.
PD MAR 15
PY 2013
VL 130
BP 121
EP 135
DI 10.1016/j.rse.2012.11.015
PG 15
WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic
Technology
SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science &
Photographic Technology
GA 090VL
UT WOS:000315008000011
ER
PT J
AU Montesano, PM
Cook, BD
Sun, G
Simard, M
Nelson, RF
Ranson, KJ
Zhang, Z
Luthcke, S
AF Montesano, P. M.
Cook, B. D.
Sun, G.
Simard, M.
Nelson, R. F.
Ranson, K. J.
Zhang, Z.
Luthcke, S.
TI Achieving accuracy requirements for forest biomass mapping: A spaceborne
data fusion method for estimating forest biomass and LiDAR sampling
error
SO REMOTE SENSING OF ENVIRONMENT
LA English
DT Article
DE LiDAR; Biomass; Sampling error; SAR; Data fusion
ID CANOPY HEIGHT; VEGETATION STRUCTURE; BOREAL FOREST; ETM PLUS; RADAR;
INTEGRATION; ATTRIBUTES; VARIABLES; TERRAIN; MISSION
AB The synergistic use of active and passive remote sensing (i.e., data fusion) demonstrates the ability of spaceborne light detection and ranging (LiDAR), synthetic aperture radar (SAR) and multispectral imagery for achieving the accuracy requirements of a global forest biomass mapping mission (+20 Mg ha(-1) or 20%, the greater of the two, for at least 80% of grid cells). A data fusion approach also provides a means to extend 3D information from discrete spaceborne LiDAR measurements of forest structure across scales much larger than that of the LiDAR footprint. For estimating biomass, these measurements mix a number of errors including those associated with LiDAR footprint sampling over regional-global extents. A general framework for mapping above ground live forest biomass density (AGB) with a data fusion approach is presented and verified using data from NASA field campaigns near Howland, ME, USA, to assess AGB and LiDAR sampling errors across a regionally representative landscape. We combined SAR and Landsat-derived optical (passive optical) image data to identify contiguous areas (>0.5 ha) that are relatively homogenous in remote sensing metrics (forest patches). We used this image-derived data with simulated spaceborne LiDAR derived from orbit and cloud cover simulations and airborne data from NASA's Laser Vegetation Imaging Sensor (LVIS) to compute AGB and estimate LiDAR sampling error for forest patches and 100 m, 250 m, 500 m, and 1 km grid cells. At both the patch and grid scales, we evaluated differences in AGB estimation and sampling error from the combined use of LiDAR with both SAR and passive optical and with either SAR or passive optical alone. First, this data fusion approach demonstrates that incorporating forest patches into the AGB mapping framework can provide sub-grid forest information for coarser grid-level AGB reporting. Second, a data fusion approach for estimating AGB using simulated spaceborne LiDAR with SAR and passive optical image combinations reduced forest AGB sampling errors 12%-38% from those where LiDAR is used with SAR or passive optical alone. In absolute terms, sampling errors were reduced from 14-40 Mg ha(-1) to 11-28 Mg ha(-1) across all grid scales and prediction methods, where minimum sampling errors were 11, 15, 18, and 22 Mg ha(-1) for 1 km, 500 m, 250 m, and 100 m grid scales, respectively. Third, spaceborne global scale accuracy requirements were achieved whereby at least 80% of the grid cells at 100 m, 250 m, 500 m, and 1 km grid levels met AGB accuracy requirements using a combination of passive optical and SAR along with machine learning methods to predict vegetation structure metrics for forested areas without LiDAR samples. Finally, using either passive optical or SAR, accuracy requirements were met at the 500 m and 250 m grid level, respectively. (C) 2012 Elsevier Inc. All rights reserved.
C1 [Montesano, P. M.] Sigma Space Corp, Lanham, MD 20706 USA.
[Montesano, P. M.; Cook, B. D.; Nelson, R. F.; Ranson, K. J.; Luthcke, S.] NASA, Goddard Space Flight Ctr, Biospher Sci Branch, Greenbelt, MD 20771 USA.
[Montesano, P. M.; Sun, G.; Zhang, Z.] Univ Maryland, Dept Geog Sci, College Pk, MD 20742 USA.
[Simard, M.] CALTECH, Jet Prop Lab, Radar & Engn Sect, Pasadena, CA USA.
RP Montesano, PM (reprint author), NASA, Goddard Space Flight Ctr, Biospher Sci Branch, Code 618, Greenbelt, MD 20771 USA.
EM Paul.M.Montesano@nasa.gov
RI Simard, Marc/H-3516-2013; chen, zhu/K-5923-2013; Cook,
Bruce/M-4828-2013; Ranson, Kenneth/G-2446-2012; Beckley,
Matthew/D-4547-2013; Nelson, Ross/H-8266-2014
OI Simard, Marc/0000-0002-9442-4562; Cook, Bruce/0000-0002-8528-000X;
Ranson, Kenneth/0000-0003-3806-7270;
FU NASA's Terrestrial Ecology Program
FX We would like to acknowledge the work of Bryan Blair and his team at
NASA GSFC for providing the LVIS data used in this study. We also thank
the anonymous reviewers whose comments and feedback strengthened this
manuscript considerably. This work was supported by NASA's Terrestrial
Ecology Program.
NR 63
TC 18
Z9 22
U1 3
U2 96
PU ELSEVIER SCIENCE INC
PI NEW YORK
PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA
SN 0034-4257
J9 REMOTE SENS ENVIRON
JI Remote Sens. Environ.
PD MAR 15
PY 2013
VL 130
BP 153
EP 170
DI 10.1016/j.rse.2012.11.016
PG 18
WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic
Technology
SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science &
Photographic Technology
GA 090VL
UT WOS:000315008000013
ER
PT J
AU Swenson, LJ
Day, PK
Eom, BH
Leduc, HG
Llombart, N
McKenney, CM
Noroozian, O
Zmuidzinas, J
AF Swenson, L. J.
Day, P. K.
Eom, B. H.
Leduc, H. G.
Llombart, N.
McKenney, C. M.
Noroozian, O.
Zmuidzinas, J.
TI Operation of a titanium nitride superconducting microresonator detector
in the nonlinear regime
SO JOURNAL OF APPLIED PHYSICS
LA English
DT Article
ID KINETIC INDUCTANCE DETECTORS; ARRAYS; MILLIMETER; REDUCTION; RESONATOR
AB If driven sufficiently strongly, superconducting microresonators exhibit nonlinear behavior including response bifurcation. This behavior can arise from a variety of physical mechanisms including heating effects, grain boundaries or weak links, vortex penetration, or through the intrinsic nonlinearity of the kinetic inductance. Although microresonators used for photon detection are usually driven fairly hard in order to optimize their sensitivity, most experiments to date have not explored detector performance beyond the onset of bifurcation. Here, we present measurements of a lumped-element superconducting microresonator designed for use as a far-infrared detector and operated deep into the nonlinear regime. The 1 GHz resonator was fabricated from a 22 nm thick titanium nitride film with a critical temperature of 2K and a normal-state resistivity of 100 mu Omega cm. We measured the response of the device when illuminated with 6.4 pW optical loading using microwave readout powers that ranged from the low-power, linear regime to 18 dB beyond the onset of bifurcation. Over this entire range, the nonlinear behavior is well described by a nonlinear kinetic inductance. The best noise-equivalent power of 2 x 10(-16) W/Hz(1/2) at 10 Hz was measured at the highest readout power, and represents a similar to 10 fold improvement compared with operating below the onset of bifurcation. (C) 2013 American Institute of Physics. [http://dx.doi.org/10.1063/1.4794808]
C1 [Swenson, L. J.; Eom, B. H.; McKenney, C. M.; Zmuidzinas, J.] CALTECH, Div Phys Math & Astron, Pasadena, CA 91125 USA.
[Swenson, L. J.; Day, P. K.; Leduc, H. G.; Zmuidzinas, J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Llombart, N.] Delft Univ Technol, NL-2628 CD Delft, Netherlands.
[Noroozian, O.] NIST, Quantum Sensors Grp, Boulder, CO 80305 USA.
RP Swenson, LJ (reprint author), CALTECH, Div Phys Math & Astron, Pasadena, CA 91125 USA.
EM swenson@astro.caltech.edu
RI Noroozian, Omid/G-3519-2011
OI Noroozian, Omid/0000-0002-9904-1704
FU Keck Institute for Space Science; Gordon and Betty Moore Foundation
FX The authors wish to thank Teun Klapwijk and David Moore for useful
discussions relating to this work. This work was supported in part by
the Keck Institute for Space Science, the Gordon and Betty Moore
Foundation. Part of this research was carried out at the Jet Propulsion
Laboratory (JPL), California Institute of Technology, under a contract
with the National Aeronautics and Space Administration. The devices used
in this work were fabricated at the JPL Microdevices Laboratory. L.
Swenson acknowledges the support from the NASA Postdoctoral Program. L.
Swenson and C. McKenney acknowledge funding from the Keck Institute for
Space Science. (C) 2012. All rights reserved.
NR 45
TC 25
Z9 25
U1 2
U2 28
PU AMER INST PHYSICS
PI MELVILLE
PA CIRCULATION & FULFILLMENT DIV, 2 HUNTINGTON QUADRANGLE, STE 1 N O 1,
MELVILLE, NY 11747-4501 USA
SN 0021-8979
J9 J APPL PHYS
JI J. Appl. Phys.
PD MAR 14
PY 2013
VL 113
IS 10
AR 104501
DI 10.1063/1.4794808
PG 9
WC Physics, Applied
SC Physics
GA 112BC
UT WOS:000316565600059
ER
PT J
AU Zahraei, A
Hsu, KL
Sorooshian, S
Gourley, JJ
Hong, Y
Behrangi, A
AF Zahraei, Ali
Hsu, Kuo-lin
Sorooshian, Soroosh
Gourley, Jonathan J.
Hong, Yang
Behrangi, Ali
TI Short-term quantitative precipitation forecasting using an object-based
approach
SO JOURNAL OF HYDROLOGY
LA English
DT Article
DE Short-term quantitative precipitation; forecasting; Nowcasting; Storm
tracking
ID CONTINENTAL RADAR IMAGES; MESOSCALE CONVECTIVE SYSTEMS; SATELLITE
INFRARED IMAGERY; NEURAL-NETWORK; RAINFALL ESTIMATION; TRACKING
ALGORITHM; SCALE-DEPENDENCE; LIFE-CYCLE; METHODOLOGY; PREDICTABILITY
AB Short-term Quantitative Precipitation Forecasting (SQPF) is critical for flash-flood warning, navigation safety, and many other applications. The current study proposes a new object-based method, named PERCAST (PERsiann-ForeCAST), to identify, track, and nowcast storms. PERCAST predicts the location and rate of rainfall up to 4 h using the most recent storm images to extract storm features, such as advection field and changes in storm intensity and size. PERCAST is coupled with a previously developed precipitation retrieval algorithm called PERSIANN-CCS (Precipitation Estimation from Remotely Sensed Information using Artificial Neural Networks-Cloud Classification System) to forecast rainfall rates. Four case studies have been presented to evaluate the performance of the models. While the first two case studies justify the model capabilities in nowcasting single storms, the third and fourth case studies evaluate the proposed model over the contiguous US during the summer of 2010. The results show that, by considering storm Growth and Decay (GD) trends for the prediction, the PERCAST-GD further improves the predictability of convection in terms of verification parameters such as Probability of Detection (POD) and False Alarm Ratio (FAR) up to 15-20%, compared to the comparison algorithms such as PERCAST. (C) 2012 Elsevier B.V. All rights reserved.
C1 [Zahraei, Ali; Hsu, Kuo-lin; Sorooshian, Soroosh] Univ Calif Irvine, Dept Civil & Environm Engn, Henry Samueli Sch Engn, CHRS, Irvine, CA 92697 USA.
[Gourley, Jonathan J.] NOAA, Natl Severe Storms Lab, Norman, OK 73072 USA.
[Hong, Yang] Univ Oklahoma, Dept Civil Engn & Environm Sci, Atmospher Radar Res Ctr, Norman, OK 73019 USA.
[Behrangi, Ali] Calif Inst Technol Climate Ocean & Earth Sci, NASA, Jet Prop Lab, Pasadena, CA USA.
RP Zahraei, A (reprint author), NOAA CREST, Washington, DC USA.
EM azahraei@ccny.cuny.edu; kuolinh@uci.edu; soroosh@uci.edu;
Jj.Gourley@noaa.gov; yanghon-g@ou.edu; ali.behrangi@jpl.nasa.gov
RI Hong, Yang/D-5132-2009; sorooshian, soroosh/B-3753-2008; Gourley,
Jonathan/C-7929-2016
OI Hong, Yang/0000-0001-8720-242X; sorooshian, soroosh/0000-0001-7774-5113;
Gourley, Jonathan/0000-0001-7363-3755
FU Center for Hydrometeorology and Remote Sensing (CHRS) at the University
of California, Irvine; NOAA/NESDIS/NCDC [NAO9NES4400006]; NCSU CICS
[2009-1380-01]; ARO [W911NF-11-1-0422]; NASA NEWS [NNX06AF93G];
Hydrologic Research Lab of the US National Weather Service (HRL-NWS)
FX This research was supported by the Center for Hydrometeorology and
Remote Sensing (CHRS) at the University of California, Irvine. Partial
financial support was provided by NOAA/NESDIS/NCDC (prime award
NAO9NES4400006, NCSU CICS subaward 2009-1380-01), ARO (grant
W911NF-11-1-0422) and NASA NEWS (Grant NNX06AF93G). Graduate fellowship
support provided by the Hydrologic Research Lab of the US National
Weather Service (HRL-NWS) is also greatly appreciated. Part of the
research was carried out at the National Severe Storm Lab (NSSL/NOAA),
Norman, OK. The authors thank Dr. Jeff Kimpel from NSSL for providing
the opportunity for collaboration between CHRS and NSSL.
NR 50
TC 9
Z9 9
U1 1
U2 36
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0022-1694
J9 J HYDROL
JI J. Hydrol.
PD MAR 13
PY 2013
VL 483
BP 1
EP 15
DI 10.1016/j.jhydrol.2012.09.052
PG 15
WC Engineering, Civil; Geosciences, Multidisciplinary; Water Resources
SC Engineering; Geology; Water Resources
GA 111HL
UT WOS:000316512300001
ER
PT J
AU Cho, KS
Gopalswamy, N
Kwon, RY
Kim, RS
Yashiro, S
AF Cho, K. -S.
Gopalswamy, N.
Kwon, R. -Y.
Kim, R. -S.
Yashiro, S.
TI A HIGH-FREQUENCY TYPE II SOLAR RADIO BURST ASSOCIATED WITH THE 2011
FEBRUARY 13 CORONAL MASS EJECTION
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE shock waves; Sun: corona; Sun: coronal mass ejections (CMEs); Sun:
flares; Sun: fundamental parameters; Sun: radio radiation
ID X-RAY EMISSIONS; SHOCK-WAVES; MAGNETIC-FIELD; FLARES; STREAMERS;
RADIATION; DENSITY; ORIGIN; SUN
AB We examine the relationship between the high-frequency (425 MHz) type II radio burst and the associated white-light coronal mass ejection (CME) that occurred on 2011 February 13. The radio burst had a drift rate of 2.5 MHz s(-1), indicating a relatively high shock speed. From SDO/AIA observations we find that a loop-like erupting front sweeps across high-density coronal loops near the start time of the burst (17:34:17 UT). The deduced distance of shock formation (0.06 Rs) from the flare center and speed of the shock (1100 km s(-1)) using the measured density from SDO/AIA observations are comparable to the height (0.05 Rs, from the solar surface) and speed (700 km s(-1)) of the CME leading edge observed by STEREO/EUVI. We conclude that the type II burst originates even in the low corona (<59 Mm or 0.08 Rs, above the solar surface) due to the fast CME shock passing through high-density loops.
C1 [Cho, K. -S.; Kim, R. -S.] Korea Astron & Space Sci Inst, Taejon 305348, South Korea.
[Cho, K. -S.; Gopalswamy, N.; Kwon, R. -Y.; Kim, R. -S.; Yashiro, S.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Cho, K. -S.; Kwon, R. -Y.; Kim, R. -S.; Yashiro, S.] Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA.
RP Cho, KS (reprint author), Korea Astron & Space Sci Inst, Taejon 305348, South Korea.
EM kscho@kasi.re.kr
OI Gopalswamy, Nat/0000-0001-5894-9954
FU NASA LWS TRT program; "Development of Korea Space Weather Center"
project of KASI; KASI basic research fund
FX This research was supported by a NASA LWS TR&T program. National Radio
Astronomy Observatory (NRAO) is operated for the NSF by associated
universities, Inc., under a cooperative agreement. K.S.C. is indebted to
M. Aschwanden for assistance with the coronal density estimation. We
thank the referee for helpful comments, which improved the presentation
of the paper. This work was partially supported by the "Development of
Korea Space Weather Center" project of KASI and the KASI basic research
fund.
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PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD MAR 10
PY 2013
VL 765
IS 2
AR 148
DI 10.1088/0004-637X/765/2/148
PG 9
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 103MP
UT WOS:000315921500073
ER
PT J
AU Cluver, ME
Appleton, PN
Ogle, P
Jarrett, TH
Rasmussen, J
Lisenfeld, U
Guillard, P
Verdes-Montenegro, L
Antonucci, R
Bitsakis, T
Charmandaris, V
Boulanger, F
Egami, E
Xu, CK
Yun, MS
AF Cluver, M. E.
Appleton, P. N.
Ogle, P.
Jarrett, T. H.
Rasmussen, J.
Lisenfeld, U.
Guillard, P.
Verdes-Montenegro, L.
Antonucci, R.
Bitsakis, T.
Charmandaris, V.
Boulanger, F.
Egami, E.
Xu, C. K.
Yun, M. S.
TI ENHANCED WARM H-2 EMISSION IN THE COMPACT GROUP MID-INFRARED "GREEN
VALLEY"
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: evolution; galaxies: groups: general; galaxies: interactions;
galaxies: ISM; infrared: galaxies; intergalactic medium
ID SPITZER-SPACE-TELESCOPE; MOLECULAR-HYDROGEN EMISSION; EARLY-TYPE
GALAXIES; STEPHANS QUINTET; STAR-FORMATION; INFRARED-EMISSION;
SEYFERT-GALAXIES; NEUTRAL HYDROGEN; STELLAR POPULATION;
OPTICAL-PROPERTIES
AB We present results from a Spitzer mid-infrared spectroscopy study of a sample of 74 galaxies located in 23 Hickson Compact Groups (HCGs), chosen to be at a dynamically active stage of Hi depletion. We find evidence for enhanced warm H-2 emission (i.e., above that associated with UV excitation in star-forming regions) in 14 galaxies (similar to 20%), with 8 galaxies having extreme values of L(H2 S(0)-S(3))/L(7.7 mu m polycyclic aromatic hydrocarbon), in excess of 0.07. Such emission has been seen previously in the compact group HCG 92 (Stephan's Quintet), and was shown to be associated with the dissipation of mechanical energy associated with a large-scale shock caused when one group member collided, at high velocity, with tidal debris in the intragroup medium. Similarly, shock excitation or turbulent heating is likely responsible for the enhanced H-2 emission in the compact group galaxies, since other sources of heating (UV or X-ray excitation from star formation or active galactic nuclei) are insufficient to account for the observed emission. The group galaxies fall predominantly in a region of mid-infrared color-color space identified by previous studies as being connected to rapid transformations in HCG galaxy evolution. Furthermore, the majority of H-2-enhanced galaxies lie in the optical "green valley" between the blue cloud and red sequence, and are primarily early-type disk systems. We suggest that H-2-enhanced systems may represent a specific phase in the evolution of galaxies in dense environments and provide new insight into mechanisms which transform galaxies onto the optical red sequence.
C1 [Cluver, M. E.; Ogle, P.; Guillard, P.] CALTECH, IPAC, Spitzer Sci Ctr, Pasadena, CA 91125 USA.
[Cluver, M. E.; Xu, C. K.] Australian Astron Observ, N Ryde, NSW 1670, Australia.
[Appleton, P. N.] CALTECH, NASA, Herschel S Ctr, Pasadena, CA 91125 USA.
[Jarrett, T. H.] Univ Cape Town, Dept Astron, ZA-7701 Rondebosch, South Africa.
[Rasmussen, J.] Univ Copenhagen, Niels Bohr Inst, Dark Cosmol Ctr, DK-2100 Copenhagen, Denmark.
[Lisenfeld, U.] Univ Granada, Fac Ciencias, Dept Fis Teor & Cosmos, E-18071 Granada, Spain.
[Verdes-Montenegro, L.] CSIC, IAA, E-18080 Granada, Spain.
[Antonucci, R.] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA.
[Bitsakis, T.; Charmandaris, V.] Univ Crete, Dept Phys, GR-71003 Iraklion, Greece.
[Charmandaris, V.] Fdn Res & Technol Hellas, IESL, GR-71110 Iraklion, Greece.
[Charmandaris, V.] Observ Paris, F-75014 Paris, France.
[Boulanger, F.] Univ Paris 11, Inst Astrophys Spatiale, Orsay, France.
[Egami, E.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA.
[Yun, M. S.] Univ Massachusetts, Dept Astron, Amherst, MA 01003 USA.
EM mcluver@aao.gov.au
RI Charmandaris, Vassilis/A-7196-2008; Lisenfeld, Ute/A-1637-2015;
Bitsakis, Theodoros/O-2766-2013;
OI Charmandaris, Vassilis/0000-0002-2688-1956; Lisenfeld,
Ute/0000-0002-9471-5423; Bitsakis, Theodoros/0000-0001-5787-8242;
Rasmussen, Jesper/0000-0002-3947-1518; Appleton,
Philip/0000-0002-7607-8766; Cluver, Michelle/0000-0002-9871-6490
FU Australian Research Council [FS110200023]; NASa, JPL/Caltech; Spanish
Ministerio de Ciencia y Educacion [AYA2007-67625-C02-02, AYA2011-24728];
Junta de Andalucia (Spain) [FQM108, P08-FQM-4205, TIC-114]; MICINN fund;
FEDER fund; National Aeronautics and Space Administration;
[AYA2008-06181-C02]; [AYA2011-30491-C02-01]
FX We thank the referee for helpful comments and suggestions that improved
the content and clarity of this paper. We are grateful to Sanch
Borthakur (Johns Hopkins University) for access to unpublished Hi data
and Michael Brown (Monash University) for the use of his galaxy template
library. This work is based on observations made with the Spitzer Space
Telescope, which is operated by the Jet Propulsion Laboratory,
California Institute of Technology under NASA contract 1407. M.E.C.
acknowledges support from the Australian Research Council (FS110200023).
Support for this work was provided by NASA through an award issued by
JPL/Caltech. U.L. acknowledges support by the research projects
AYA2007-67625-C02-02 and AYA2011-24728 from the Spanish Ministerio de
Ciencia y Educacion and the Junta de Andalucia (Spain) grant FQM108.
L.V.M. is funded by grants AYA2008-06181-C02 and AYA2011-30491-C02-01,
co-financed by MICINN and FEDER funds, and the Junta de Andalucia
(Spain) grants P08-FQM-4205 and TIC-114. This research has made use of
the NASA/IPAC Extragalactic Database (NED) which is operated by the Jet
Propulsion Laboratory, California Institute of Technology, under
contract with the National Aeronautics and Space Administration. This
research has made use of data obtained from the Chandra Source Catalog,
provided by the Chandra X-ray Center (CXC) as part of the Chandra Data
Archive.
NR 97
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PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD MAR 10
PY 2013
VL 765
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AR 93
DI 10.1088/0004-637X/765/2/93
PG 29
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 103MP
UT WOS:000315921500018
ER
PT J
AU Contopoulos, I
Kazanas, D
Papadopoulos, DB
AF Contopoulos, Ioannis
Kazanas, Demosthenes
Papadopoulos, Demetrios B.
TI THE FORCE-FREE MAGNETOSPHERE OF A ROTATING BLACK HOLE
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE accretion; accretion disks-black hole physics-magnetohydrodynamics(MHD)
ID PULSAR MAGNETOSPHERE; ELECTRODYNAMICS; RADIATION; BINARIES; GEOMETRY;
SYSTEM; SPIN
AB We revisit the Blandford-Znajek process and solve the fundamental equation that governs the structure of the steady-state force-free magnetosphere around a Kerr black hole. The solution depends on the distributions of the magnetic field angular velocity. and the poloidal electric current I. These are not arbitrary. They are determined self-consistently by requiring that magnetic field lines cross smoothly the two singular surfaces of the problem: the inner "light surface" located inside the ergosphere and the outer "light surface" which is the generalization of the pulsar light cylinder. We find the solution for the simplest possible magnetic field configuration, the split monopole, through a numerical iterative relaxation method analogous to the one that yields the structure of the steady-state axisymmetric force-free pulsar magnetosphere. We obtain the rate of electromagnetic extraction of energy and confirm the results of Blandford and Znajek and of previous time- dependent simulations. Furthermore, we discuss the physical applicability of magnetic field configurations that do not cross both " light surfaces."
C1 [Contopoulos, Ioannis] Acad Athens, Res Ctr Astron, Athens 11527, Greece.
[Kazanas, Demosthenes] NASA, GSFC, Greenbelt, MD 20771 USA.
[Papadopoulos, Demetrios B.] Aristotle Univ Thessaloniki, Dept Phys, Thessaloniki 54124, Greece.
RP Contopoulos, I (reprint author), Acad Athens, Res Ctr Astron, Athens 11527, Greece.
EM icontop@academyofathens.gr; demos.kazanas@nasa.gov;
papadop@astro.auth.gr
FU General Secretariat for Research and Technology of Greece; European
Social Fund
FX We thank Professors George Contopoulos and Maxim Lyutikov for
interesting discussions. This work was supported by the General
Secretariat for Research and Technology of Greece and the European
Social Fund in the framework of Action "Excellence."
NR 29
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PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD MAR 10
PY 2013
VL 765
IS 2
AR 113
DI 10.1088/0004-637X/765/2/113
PG 6
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 103MP
UT WOS:000315921500038
ER
PT J
AU Dzyurkevich, N
Turner, NJ
Henning, T
Kley, W
AF Dzyurkevich, Natalia
Turner, Neal J.
Henning, Thomas
Kley, Wilhelm
TI MAGNETIZED ACCRETION AND DEAD ZONES IN PROTOSTELLAR DISKS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE accretion; accretion disks-circumstellar
matter-instabilitiesmagnetohydrodynamics(MHD)-protoplanetarydisks
ID DIFFUSE INTERSTELLAR CLOUDS; 3-DIMENSIONAL MAGNETOHYDRODYNAMIC
SIMULATIONS; TURBULENT PROTOPLANETARY DISCS; GLOBAL MHD SIMULATIONS;
YOUNG STELLAR OBJECTS; WEAKLY IONIZED DISKS; RAY IONIZATION RATE; T
TAURI DISKS; MAGNETOROTATIONAL INSTABILITY; NONLINEAR EVOLUTION
AB The edges of magnetically dead zones in protostellar disks have been proposed as locations where density bumps may arise, trapping planetesimals and helping form planets. Magneto-rotational turbulence in magnetically active zones provides both accretion of gas on the star and transport of mass to the dead zone. We investigate the location of the magnetically active regions in a protostellar disk around a solar-type star, varying the disk temperature, surface density profile, and dust-to-gas ratio. We also consider stellar masses between 0.4 and 2M(circle dot), with corresponding adjustments in the disk mass and temperature. The dead zone's size and shape are found using the Elsasser number criterion with conductivities including the contributions from ions, electrons, and charged fractal dust aggregates. The charged species' abundances are found using the approach proposed by Okuzumi. The dead zone is in most cases defined by the ambipolar diffusion. In our maps, the dead zone takes a variety of shapes, including a fish tail pointing away from the star and islands located on and off the midplane. The corresponding accretion rates vary with radius, indicating locations where the surface density will increase over time, and others where it will decrease. We show that density bumps do not readily grow near the dead zone's outer edge, independently of the disk parameters and the dust properties. Instead, the accretion rate peaks at the radius where the gas-phase metals freeze out. This could lead to clearing a valley in the surface density, and to a trap for pebbles located just outside the metal freezeout line.
C1 [Dzyurkevich, Natalia; Henning, Thomas] Max Planck Inst Astron, D-69117 Heidelberg, Germany.
[Dzyurkevich, Natalia] Ecole Normale Super, CNRS, Lab Radioastron, UMR 8112, F-75231 Paris 05, France.
[Dzyurkevich, Natalia] Observ Paris, F-75231 Paris 05, France.
[Turner, Neal J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Kley, Wilhelm] Univ Tubingen, Inst Astron & Astrophys, Dept Computat Phys, D-72076 Tubingen, Germany.
RP Dzyurkevich, N (reprint author), Max Planck Inst Astron, Konigstuhl 17, D-69117 Heidelberg, Germany.
RI Kley, Wilhelm/A-4921-2012;
OI Turner, Neal/0000-0001-8292-1943
FU Deutsche Forschungsgemeinschaft (DFG) [Forschergruppe 759]; NASA Solar
Systems Origins program [07-SSO07-0044]; Alexander von Humboldt
Foundation; Deutsches Zentrum fur Luft-und Raumfahrt (DLR) [50 OR 0401]
FX N. Dzyurkevich was supported by the Deutsche Forschungsgemeinschaft
(DFG) through Forschergruppe 759, "The Formation of Planets: The
Critical First Growth Phase." We acknowledge support from the Deutsches
Zentrum fur Luft-und Raumfahrt (DLR), support code 50 OR 0401. N.J.
Turner's participation was supported by the NASA Solar Systems Origins
program under grant 07-SSO07-0044, and by the Alexander von Humboldt
Foundation through a Fellowship for Experienced Researchers. The work
was carried out in part at the Jet Propulsion Laboratory, California
Institute of Technology. We thank ProfessorW. Brandner and M. Gennaro
for the tutoring on the STELLAR code. We thank S. Okuzumi for a very
thorough referee report that greatly improved the quality of this paper.
NR 100
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD MAR 10
PY 2013
VL 765
IS 2
AR 114
DI 10.1088/0004-637X/765/2/114
PG 27
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 103MP
UT WOS:000315921500039
ER
PT J
AU Hathi, NP
Cohen, SH
Ryan, RE
Finkelstein, SL
McCarthy, PJ
Windhorst, RA
Yan, H
Koekemoer, AM
Rutkowski, MJ
O'Connell, RW
Straughn, AN
Balick, B
Bond, HE
Calzetti, D
Disney, MJ
Dopita, MA
Frogel, JA
Hall, DNB
Holtzman, JA
Kimble, RA
Paresce, F
Saha, A
Silk, JI
Trauger, JT
Walker, AR
Whitmore, BC
Young, ET
AF Hathi, N. P.
Cohen, S. H.
Ryan, R. E., Jr.
Finkelstein, S. L.
McCarthy, P. J.
Windhorst, R. A.
Yan, H.
Koekemoer, A. M.
Rutkowski, M. J.
O'Connell, R. W.
Straughn, A. N.
Balick, B.
Bond, H. E.
Calzetti, D.
Disney, M. J.
Dopita, M. A.
Frogel, Jay A.
Hall, D. N. B.
Holtzman, J. A.
Kimble, R. A.
Paresce, F.
Saha, A.
Silk, J. I.
Trauger, J. T.
Walker, A. R.
Whitmore, B. C.
Young, E. T.
TI STELLAR POPULATIONS OF LYMAN BREAK GALAXIES AT z similar or equal to 1-3
IN THE HST/WFC3 EARLY RELEASE SCIENCE OBSERVATIONS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: evolution; galaxies: fundamental parameters; galaxies:
high-redshift; ultraviolet: galaxies
ID STAR-FORMING GALAXIES; HIGH-REDSHIFT GALAXIES; ULTRA-DEEP-FIELD;
GOODS-SOUTH FIELD; COSMOLOGICAL HYDRODYNAMIC SIMULATIONS; EXTRAGALACTIC
LEGACY SURVEY; REST-FRAME ULTRAVIOLET; UV LUMINOSITY FUNCTION;
PHOTOMETRIC REDSHIFTS; FORMATION HISTORIES
AB We analyze the spectral energy distributions (SEDs) of Lyman break galaxies (LBGs) at z similar or equal to 1-3 selected using the Hubble Space Telescope (HST) Wide Field Camera 3 (WFC3) UVIS channel filters. These HST/WFC3 observations cover about 50 arcmin(2) in the GOODS-South field as a part of the WFC3 Early Release Science program. These LBGs at z similar or equal to 1-3 are selected using dropout selection criteria similar to high-redshift LBGs. The deep multi-band photometry in this field is used to identify best-fit SED models, from which we infer the following results: (1) the photometric redshift estimate of these dropout-selected LBGs is accurate to within few percent; (2) the UV spectral slope beta is redder than at high redshift (z > 3), where LBGs are less dusty; (3) on average, LBGs at z similar or equal to 1-3 are massive, dustier, and more highly star forming, compared to LBGs at higher redshifts with similar luminosities (0.1L* less than or similar to L less than or similar to 2.5L*), though their median values are similar within 1 sigma uncertainties. This could imply that identical dropout selection technique, at all redshifts, finds physically similar galaxies; and (4) the stellar masses of these LBGs are directly proportional to their UV luminosities with a logarithmic slope of similar to 0.46, and star formation rates are proportional to their stellar masses with a logarithmic slope of similar to 0.90. These relations hold true-within luminosities probed in this study-for LBGs from z similar or equal to 1.5 to 5. The star-forming galaxies selected using other color-based techniques show similar correlations at z similar or equal to 2, but to avoid any selection biases, and for direct comparison with LBGs at z > 3, a true Lyman break selection at z similar or equal to 2 is essential. The future HST UV surveys, both wider and deeper, covering a large luminosity range are important to better understand LBG properties and their evolution.
C1 [Hathi, N. P.; McCarthy, P. J.] Observ Carnegie Inst Sci, Pasadena, CA 91101 USA.
[Cohen, S. H.; Windhorst, R. A.; Rutkowski, M. J.] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85287 USA.
[Ryan, R. E., Jr.; Koekemoer, A. M.; Bond, H. E.; Whitmore, B. C.] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
[Finkelstein, S. L.] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA.
[Yan, H.] Univ Missouri, Dept Phys & Astron, Columbia, MO 65211 USA.
[O'Connell, R. W.] Univ Virginia, Dept Astron, Charlottesville, VA 22904 USA.
[Straughn, A. N.; Kimble, R. A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Balick, B.] Univ Washington, Dept Astron, Seattle, WA 98195 USA.
[Calzetti, D.] Univ Massachusetts, Dept Astron, Amherst, MA 01003 USA.
[Disney, M. J.] Cardiff Univ, Sch Phys & Astron, Cardiff CF24 3AA, S Glam, Wales.
[Dopita, M. A.] Australian Natl Univ, Res Sch Astron & Astrophys, Weston, ACT 2611, Australia.
[Dopita, M. A.; Frogel, Jay A.] King Abdulaziz Univ, Dept Astron, Jeddah 21413, Saudi Arabia.
[Frogel, Jay A.] Galaxies Unltd, Lutherville Timonium, MD 21093 USA.
[Hall, D. N. B.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA.
[Holtzman, J. A.] New Mexico State Univ, Dept Astron, Las Cruces, NM 88003 USA.
[Paresce, F.] INAF, Ist Astrofis Spaziale & Fis Cosm, I-40129 Bologna, Italy.
[Saha, A.] Natl Opt Astron Observ, Tucson, AZ 85726 USA.
[Silk, J. I.] Univ Oxford, Dept Phys, Oxford OX1 3PU, England.
[Trauger, J. T.] NASA, Jet Prop Lab, Pasadena, CA 91109 USA.
[Walker, A. R.] Cerro Tololo Interamer Observ, La Serena, Chile.
[Young, E. T.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
RP Hathi, NP (reprint author), Observ Carnegie Inst Sci, Pasadena, CA 91101 USA.
EM nhathi@obs.carnegiescience.edu
RI Dopita, Michael/P-5413-2014; Hathi, Nimish/J-7092-2014;
OI Dopita, Michael/0000-0003-0922-4986; Hathi, Nimish/0000-0001-6145-5090;
Koekemoer, Anton/0000-0002-6610-2048
FU NASA through Space Telescope Science Institute [11359,
HST-GO-11359.08-A]; NASA [NAS 5-26555]; STScI/NASA [HST-GO-12286.02-A];
American Astronomical Society
FX We thank the referee for helpful comments and suggestions that
significantly improved this paper. This paper is based on Early Release
Science observations made by the WFC3 Scientific Oversight Committee. We
are grateful to the Director of the Space Telescope Science Institute
for awarding Director's Discretionary time for this program. Support for
program 11359 was provided by NASA through a grant HST-GO-11359.08-A
from the Space Telescope Science Institute, which is operated by the
Association of Universities for Research in Astronomy, Inc., under NASA
contract NAS 5-26555. N.P.H. also acknowledges support provided by
STScI/NASA grant HST-GO-12286.02-A. This research was (partially)
supported by a grant from the American Astronomical Society.
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD MAR 10
PY 2013
VL 765
IS 2
AR 88
DI 10.1088/0004-637X/765/2/88
PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 103MP
UT WOS:000315921500013
ER
PT J
AU Kaiser, RI
Stockton, AM
Kim, YS
Jensen, EC
Mathies, RA
AF Kaiser, R. I.
Stockton, A. M.
Kim, Y. S.
Jensen, E. C.
Mathies, R. A.
TI ON THE FORMATION OF DIPEPTIDES IN INTERSTELLAR MODEL ICES
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE astrobiology-astrochemistry -cosmic rays-ISM; molecules-methods;
laboratory-Online-only material; color figures
ID COSMIC-RAY PARTICLES; AMINO-ACIDS; CARBONACEOUS CHONDRITES; ANALOGS;
IRRADIATION; CHEMISTRY; PEPTIDES; ORIGIN; ISOMER; EARTH
AB The hypothesis of an exogenous origin and delivery of biologically important molecules to early Earth presents an alternative route to their terrestrial in situ formation. Dipeptides like Gly-Gly detected in the Murchison meteorite are considered as key molecules in prebiotic chemistry because biofunctional dipeptides present the vital link in the evolutionary transition from prebiotic amino acids to early proteins. However, the processes that could lead to the exogenous abiotic synthesis of dipeptides are unknown. Here, we report the identification of two proteinogenic dipeptides-Gly-Gly and Leu-Ala-formed via electron-irradiation of interstellar model ices followed by annealing the irradiated samples to 300 K. Our results indicate that the radiation-induced, non- enzymatic formation of proteinogenic dipeptides in interstellar ice analogs is facile. Once synthesized and incorporated into the "building material" of solar systems, biomolecules at least as complex as dipeptides could have been delivered to habitable planets such as early Earth by meteorites and comets, thus seeding the beginning of life as we know it.
C1 [Kaiser, R. I.; Kim, Y. S.] Univ Hawaii Manoa, Dept Chem, Honolulu, HI 96822 USA.
[Stockton, A. M.; Jensen, E. C.; Mathies, R. A.] Univ Calif Berkeley, Dept Chem, Berkeley, CA 94720 USA.
[Stockton, A. M.] Jet Prop Lab, Pasadena, CA 91109 USA.
RP Kaiser, RI (reprint author), Univ Hawaii Manoa, Dept Chem, Honolulu, HI 96822 USA.
FU US National Science Foundation "Collaborative Research in Chemistry
Program" (NSF-CRC) [CHE-0627854]; Mathies Royalty Fund
FX We thank Professor P. B. Price (UC Berkeley, Physics Department) and Dr.
Max Bernstein (NASA) for helpful comments and discussions and Dr. Thomas
Chiesl (UC Berkeley) for his assistance in the initial phase of the
project. Microdevices were fabricated in the UC Berkeley
Bionanotechnology Center. This work was supported by the US National
Science Foundation "Collaborative Research in Chemistry Program"
(NSF-CRC; CHE-0627854). Research at Berkeley was supported by the
Mathies Royalty Fund.
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PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD MAR 10
PY 2013
VL 765
IS 2
AR 111
DI 10.1088/0004-637X/765/2/111
PG 9
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 103MP
UT WOS:000315921500036
ER
PT J
AU Kopparapu, RK
Ramirez, R
Kasting, JF
Eymet, V
Robinson, TD
Mahadevan, S
Terrien, RC
Domagal-Goldman, S
Meadows, V
Deshpande, R
AF Kopparapu, Ravi Kumar
Ramirez, Ramses
Kasting, James F.
Eymet, Vincent
Robinson, Tyler D.
Mahadevan, Suvrath
Terrien, Ryan C.
Domagal-Goldman, Shawn
Meadows, Victoria
Deshpande, Rohit
TI HABITABLE ZONES AROUND MAIN-SEQUENCE STARS: NEW ESTIMATES
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE planetary systems
ID EARTH-LIKE PLANETS; MOLECULAR SPECTROSCOPIC DATABASE; CARBON-DIOXIDE
CLOUDS; EARLY MARTIAN CLIMATE; ORBITING M-DWARFS; HIGH-LEVEL CLOUDS;
M-CIRCLE-PLUS; EARLY MARS; EXTRASOLAR PLANETS; RADIATIVE-TRANSFER
AB Identifying terrestrial planets in the habitable zones (HZs) of other stars is one of the primary goals of ongoing radial velocity (RV) and transit exoplanet surveys and proposed future space missions. Most current estimates of the boundaries of the HZ are based on one-dimensional (1D), cloud-free, climate model calculations by Kasting et al. However, this model used band models that were based on older HITRAN and HITEMP line-by-line databases. The inner edge of the HZ in the Kasting et al. model was determined by loss of water, and the outer edge was determined by the maximum greenhouse provided by a CO2 atmosphere. A conservative estimate for the width of the HZ from this model in our solar system is 0.95-1.67 AU. Here an updated 1D radiative-convective, cloud-free climate model is used to obtain new estimates for HZ widths around F, G, K, and M stars. New H2O and CO2 absorption coefficients, derived from the HITRAN 2008 and HITEMP 2010 line-by-line databases, are important improvements to the climate model. According to the new model, the water-loss (inner HZ) and maximum greenhouse (outer HZ) limits for our solar system are at 0.99 and 1.70 AU, respectively, suggesting that the present Earth lies near the inner edge. Additional calculations are performed for stars with effective temperatures between 2600 and 7200 K, and the results are presented in parametric form, making them easy to apply to actual stars. The new model indicates that, near the inner edge of the HZ, there is no clear distinction between runaway greenhouse and water-loss limits for stars with T-eff less than or similar to 5000 K, which has implications for ongoing planet searches around K and M stars. To assess the potential habitability of extrasolar terrestrial planets, we propose using stellar flux incident on a planet rather than equilibrium temperature. This removes the dependence on planetary (Bond) albedo, which varies depending on the host star's spectral type. We suggest that conservative estimates of the HZ (water-loss and maximum greenhouse limits) should be used for current RV surveys and Kepler mission to obtain a lower limit on.., so that future flagship missions like TPF-C and Darwin are not undersized. Our model does not include the radiative effects of clouds; thus, the actual HZ boundaries may extend further in both directions than the estimates just given.
C1 [Kopparapu, Ravi Kumar; Ramirez, Ramses; Kasting, James F.] Penn State Univ, Dept Geosci, University Pk, PA 16802 USA.
[Kopparapu, Ravi Kumar; Ramirez, Ramses; Kasting, James F.] Penn State Astrobiol Res Ctr, University Pk, PA 16802 USA.
[Kopparapu, Ravi Kumar; Ramirez, Ramses; Kasting, James F.; Mahadevan, Suvrath; Terrien, Ryan C.; Deshpande, Rohit] Penn State Univ, Ctr Exoplanets & Habitable Worlds, University Pk, PA 16802 USA.
[Eymet, Vincent] Univ Bordeaux 1, UMR 5804, Lab Astrophys Bordeaux, F-33270 Floirac, France.
[Robinson, Tyler D.; Meadows, Victoria] Univ Washington, Dept Astron, Seattle, WA 98195 USA.
[Robinson, Tyler D.] Univ Washington, Astrobiol Program, Seattle, WA 98195 USA.
[Mahadevan, Suvrath; Terrien, Ryan C.; Deshpande, Rohit] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA.
[Domagal-Goldman, Shawn] NASA Goddard Space Flight Ctr, Planetary Environm Lab, Greenbelt, MD USA.
RP Kopparapu, RK (reprint author), Penn State Univ, Dept Geosci, 443 Deike Bldg, University Pk, PA 16802 USA.
RI Domagal-Goldman, Shawn/F-3521-2012
OI Domagal-Goldman, Shawn/0000-0003-0354-9325
FU NASA Astrobiology Institute's Virtual Planetary Laboratory lead team;
NASA [NNH05ZDA001C]; Penn State Astrobiology Research Center; ITAAC
project (Impact du Trafic Aerien sur l'Atmosphere et le Climat);
Fondation Sciences et Technologies pour l'Aeoronautique et l'Espace
(STAE), Toulouse, France, within the Reseau Thematique de Recherche
Avancee (RTRA); European Research Council [209622: E3ARTHs]; NSF
[AST1006676, AST1126413]; PSARC; Pennsylvania State University; Eberly
College of Science; Pennsylvania Space Grant Consortium; Oak Ridge
Associated Universities NASA Postdoctoral Management Program; NASA NAI
FX R.K., R.R., J.F.K., and S.D.D.G. gratefully acknowledge funding from
NASA Astrobiology Institute's Virtual Planetary Laboratory lead team,
supported by NASA under cooperative agreement NNH05ZDA001C, and the Penn
State Astrobiology Research Center. V.E. acknowledges the support of the
ITAAC project (Impact du Trafic Aerien sur l'Atmosphere et le Climat),
funded by the Fondation Sciences et Technologies pour l'Aeoronautique et
l'Espace (STAE), Toulouse, France, within the Reseau Thematique de
Recherche Avancee (RTRA), and support from the European Research Council
(Starting Grant 209622: E3ARTHs). S. M. acknowledges support from NSF
AST1006676, AST1126413, PSARC, and the NASA NAI. The Center for
Exoplanets and Habitable Worlds is supported by the Pennsylvania State
University, the Eberly College of Science, and the Pennsylvania Space
Grant Consortium. S.D.D.G. was also supported by the Oak Ridge
Associated Universities NASA Postdoctoral Management Program and did
much of his work on this project while in residence at NASA
Headquarters.
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD MAR 10
PY 2013
VL 765
IS 2
AR 131
DI 10.1088/0004-637X/765/2/131
PG 16
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 103MP
UT WOS:000315921500056
ER
PT J
AU Lehmer, BD
Lucy, AB
Alexander, DM
Best, PN
Geach, JE
Harrison, CM
Hornschemeier, AE
Matsuda, Y
Mullaney, JR
Smail, I
Sobral, D
Swinbank, AM
AF Lehmer, B. D.
Lucy, A. B.
Alexander, D. M.
Best, P. N.
Geach, J. E.
Harrison, C. M.
Hornschemeier, A. E.
Matsuda, Y.
Mullaney, J. R.
Smail, Ian
Sobral, D.
Swinbank, A. M.
TI CONCURRENT SUPERMASSIVE BLACK HOLE AND GALAXY GROWTH: LINKING
ENVIRONMENT AND NUCLEAR ACTIVITY IN z=2.23 H alpha EMITTERS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE cosmology: observations; early universe; galaxies: active; galaxies:
clusters: general; surveys; X-rays: general
ID STAR-FORMATION RATE; SPACE-TELESCOPE OBSERVATIONS; EXTRAGALACTIC LEGACY
SURVEY; HIGH-REDSHIFT SURVEY; CHANDRA-DEEP-FIELDS; GALACTIC NUCLEI;
ELLIPTIC GALAXIES; FORMATION HISTORY; HOST GALAXIES; STELLAR-MASS
AB We present results from a approximate to 100 ks Chandra observation of the 2QZ Cluster 1004+00 structure at z = 2.23 (hereafter 2QZ Clus). 2QZ Clus was originally identified as an overdensity of four optically-selected QSOs at z = 2.23 within a 15 x 15 arcmin(2) region. Narrow-band imaging in the near-IR (within the K band) revealed that the structure contains an additional overdensity of 22 z = 2.23 H alpha-emitting galaxies (HAEs), resulting in 23 unique z = 2.23 HAEs/QSOs (22 within the Chandra field of view). Our Chandra observations reveal that three HAEs in addition to the four QSOs harbor powerfully accreting supermassive black holes (SMBHs), with 2-10 keV luminosities of approximate to(8-60) x 10(43) erg s(-1) and X-ray spectral slopes consistent with unobscured active galactic nucleus (AGN). Using a large comparison sample of 210 z = 2.23 HAEs in the Chandra-COSMOS field (C-COSMOS), we find suggestive evidence that the AGN fraction increases with local HAE galaxy density. The 2QZ Clus HAEs reside in a moderately overdense environment (a factor of approximate to 2 times over the field), and after excluding optically-selected QSOs, we find that the AGN fraction is a factor of approximate to 3.5(-2.2)(+3.8) times higher than C-COSMOS HAEs in similar environments. Using stacking analyses of the Chandra data and Herschel SPIRE observations at 250 mu m, we respectively estimate mean SMBH accretion rates ((M) over dot(BH)) and star formation rates (SFRs) for the 2QZ Clus and C-COSMOS samples. We find that the mean 2QZ Clus HAE stacked X-ray luminosity is QSO-like (L2-10 keV approximate to [6-10] x 10(43) erg s(-1)), and the implied (M) over dot(BH)/SFR approximate to(1.6-3.2) x 10(-3) is broadly consistent with the local M-BH/M-star relation and z approximate to 2 X-ray selected AGN. In contrast, the C-COSMOS HAEs are on average an order of magnitude less X-ray luminous and have (M) over dot(BH)/SFR approximate to (0.2-0.4) x 10(-3), somewhat lower than the local M-BH/M-star relation, but comparable to that found for z approximate to 1-2 star-forming galaxies with similar mean X-ray luminosities. We estimate that a periodic QSO phase with duty cycle approximate to 2%-8% would be sufficient to bring star-forming galaxies onto the local M-BH/M-star relation. This duty cycle is broadly consistent with the observed C-COSMOS HAE AGN fraction (approximate to 0.4%-2.3%) for powerful AGN with L-X greater than or similar to 10(44) erg s(-1). Future observations of 2QZ Clus will be needed to identify key factors responsible for driving the mutual growth of the SMBHs and galaxies.
C1 [Lehmer, B. D.; Hornschemeier, A. E.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA.
[Lehmer, B. D.; Lucy, A. B.; Hornschemeier, A. E.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Lucy, A. B.] Univ Oklahoma, Homer L Dodge Dept Phys & Astron, Norman, OK 73019 USA.
[Alexander, D. M.; Harrison, C. M.; Mullaney, J. R.; Swinbank, A. M.] Univ Durham, Dept Phys, Durham DH1 3LE, England.
[Best, P. N.] Royal Observ, Inst Astron, SUPA, Edinburgh EH9 3HJ, Midlothian, Scotland.
[Geach, J. E.] McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada.
[Matsuda, Y.] Natl Inst Nat Sci, Natl Astron Observ Japan, Chile Observ, Mitaka, Tokyo 1818588, Japan.
[Smail, Ian] Univ Durham, Inst Computat Cosmol, Durham DH1 3LE, England.
[Sobral, D.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands.
RP Lehmer, BD (reprint author), Johns Hopkins Univ, Dept Phys & Astron, Homewood Campus, Baltimore, MD 21218 USA.
RI Smail, Ian/M-5161-2013; Sobral, David/C-7919-2014
OI Smail, Ian/0000-0003-3037-257X; Sobral, David/0000-0001-8823-4845
FU Chandra X-ray Center [GO2-13138A]; Science and Technology Facilities
Council (STFC); Leverhulme Trust
FX We thank the anonymous referee for reviewing the manuscript and
providing helpful suggestions. We gratefully acknowledge financial
support from Chandra X-ray Center grant GO2-13138A (B.D.L., A.B.L.), the
Science and Technology Facilities Council (STFC) (I.R.S.), and the
Leverhulme Trust (I.R.S., J.R.M.).
NR 65
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD MAR 10
PY 2013
VL 765
IS 2
AR 87
DI 10.1088/0004-637X/765/2/87
PG 11
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 103MP
UT WOS:000315921500012
ER
PT J
AU McIntosh, SW
Leamon, RJ
Gurman, JB
Olive, JP
Cirtain, JW
Hathaway, DH
Burkepile, J
Miesch, M
Markel, RS
Sitongia, L
AF McIntosh, Scott W.
Leamon, Robert J.
Gurman, Joseph B.
Olive, Jean-Philippe
Cirtain, Jonathan W.
Hathaway, David H.
Burkepile, Joan
Miesch, Mark
Markel, Robert S.
Sitongia, Leonard
TI HEMISPHERIC ASYMMETRIES OF SOLAR PHOTOSPHERIC MAGNETISM: RADIATIVE,
PARTICULATE, AND HELIOSPHERIC IMPACTS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE magnetic fields; solar wind; Sun: corona
ID NORTH-SOUTH ASYMMETRY; WIND HELIUM ABUNDANCE; POLAR CORONAL HOLES; CYCLE
23; BASHFUL BALLERINA; SUNSPOT CYCLE; BRIGHT POINTS; CURRENT SHEET;
COSMIC-RAYS; EVOLUTION
AB Among many other measurable quantities, the summer of 2009 saw a considerable low in the radiative output of the Sun that was temporally coincident with the largest cosmic-ray flux ever measured at 1 AU. Combining measurements and observations made by the Solar and Heliospheric Observatory (SOHO) and Solar Dynamics Observatory (SDO) spacecraft we begin to explore the complexities of the descending phase of solar cycle 23, through the 2009 minimum into the ascending phase of solar cycle 24. A hemispheric asymmetry in magnetic activity is clearly observed and its evolution monitored and the resulting (prolonged) magnetic imbalance must have had a considerable impact on the structure and energetics of the heliosphere. While we cannot uniquely tie the variance and scale of the surface magnetism to the dwindling radiative and particulate output of the star, or the increased cosmic-ray flux through the 2009 minimum, the timing of the decline and rapid recovery in early 2010 would appear to inextricably link them. These observations support a picture where the Sun's hemispheres are significantly out of phase with each other. Studying historical sunspot records with this picture in mind shows that the northern hemisphere has been leading since the middle of the last century and that the hemispheric "dominance" has changed twice in the past 130 years. The observations presented give clear cause for concern, especially with respect to our present understanding of the processes that produce the surface magnetism in the (hidden) solar interior-hemispheric asymmetry is the normal state-the strong symmetry shown in 1996 was abnormal. Further, these observations show that the mechanism(s) which create and transport the magnetic flux are slowly changing with time and, it appears, with only loose coupling across the equator such that those asymmetries can persist for a considerable time. As the current asymmetry persists and the basal energetics of the system continue to dwindle we anticipate new radiative and particulate lows coupled with increased cosmic-ray fluxes heading into the next solar minimum.
C1 [McIntosh, Scott W.; Burkepile, Joan; Miesch, Mark; Markel, Robert S.; Sitongia, Leonard] Natl Ctr Atmospher Res, High Altitude Observ, Boulder, CO 80307 USA.
[Leamon, Robert J.] Montana State Univ, Dept Phys, Bozeman, MT 59717 USA.
[Gurman, Joseph B.] NASA, Goddard Space Flight Ctr, Solar Phys Lab, Greenbelt, MD 20771 USA.
[Olive, Jean-Philippe] Astrium SAS, F-75016 Paris, France.
[Cirtain, Jonathan W.; Hathaway, David H.] NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA.
RP McIntosh, SW (reprint author), Natl Ctr Atmospher Res, High Altitude Observ, POB 3000, Boulder, CO 80307 USA.
OI Miesch, Mark/0000-0003-1976-0811
FU National Science Foundation (NSF) grant [ATM-0925177]; NASA LWS
[NNX08AU30G, NNH08CC02C]; NASA grant [NNX08AL23G]; National Science
Foundation
FX We are grateful for comments on earlier drafts of this manuscript by
Eric Priest, Leon Golub, and Hui Tian, and S.W.M. thanks Ineke De
Moortel for her encouragement. The Oulu Neutron Monitor data were
obtained from the Sodankyla Geophysical Observatory via the Web site
http://cosmicrays.oulu.fi/. The research conducted by S.W.M. was partly
supported by the National Science Foundation (NSF) grant ATM-0925177.
S.W.M. and R.J.L. were also supported by NASA LWS grants NNX08AU30G and
NNH08CC02C. L.S., R.S.M., and S.W.M. were also partly supported by NASA
grant NNX08AL23G to produce the EIT BP database. Special thanks to
Jeneen Sommers (Stanford) for providing MDI data on request. SOHO is a
project of international collaboration between ESA and NASA to study the
Sun. We are thankful for the online publication of the KSO and SIDC
international sunspot numbers. The National Center for Atmospheric
Research is sponsored by the National Science Foundation.
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD MAR 10
PY 2013
VL 765
IS 2
AR 146
DI 10.1088/0004-637X/765/2/146
PG 17
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 103MP
UT WOS:000315921500071
ER
PT J
AU Qian, L
Li, D
Goldsmith, PF
AF Qian, Lei
Li, Di
Goldsmith, Paul F.
TI (CO)-C-13 CORES IN TAURUS MOLECULAR CLOUD (vol 760, pg 147, 2012)
SO ASTROPHYSICAL JOURNAL
LA English
DT Correction
C1 [Qian, Lei; Li, Di] Chinese Acad Sci, Natl Astron Observ, Beijing 100012, Peoples R China.
[Li, Di] Space Sci Inst, Boulder, CO USA.
[Li, Di] CALTECH, Dept Astron, Pasadena, CA 91125 USA.
[Goldsmith, Paul F.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
RP Qian, L (reprint author), Chinese Acad Sci, Natl Astron Observ, Beijing 100012, Peoples R China.
EM lqian@nao.cas.cn; ithaca.li@gmail.com
RI Goldsmith, Paul/H-3159-2016
NR 1
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD MAR 10
PY 2013
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SC Astronomy & Astrophysics
GA 103MP
UT WOS:000315921500086
ER
PT J
AU Raettig, N
Lyra, W
Klahr, H
AF Raettig, Natalie
Lyra, Wladimir
Klahr, Hubert
TI A PARAMETER STUDY FOR BAROCLINIC VORTEX AMPLIFICATION
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE accretion; accretion disks-circumstellar
matter-hydrodynamics-instabilities-methods; numerical-planetary
systems-turbulence
ID PROTOPLANETARY DISKS; ACCRETION DISKS; DEAD ZONE; MAGNETOHYDRODYNAMIC
SIMULATIONS; NUMERICAL SIMULATIONS; VORTICITY PRODUCTION; CIRCUMSTELLAR
DISKS; LINEAR-ANALYSIS; INSTABILITY; TURBULENCE
AB Recent studies have shown that baroclinic vortex amplification is strongly dependent on certain factors, namely, the global entropy gradient, the efficiency of thermal diffusion and/or relaxation as well as numerical resolution. We conduct a comprehensive study of a broad range and combination of various entropy gradients, thermal diffusion and thermal relaxation timescales via local shearing sheet simulations covering the parameter space relevant for protoplanetary disks. We measure the Reynolds stresses as a function of our control parameters and see that there is angular momentum transport even for entropy gradients as low as beta =-d ln s/d ln r=1/2. Values we expect in protoplanetary disks are between beta=0.5-2.0 The amplification-rate of the perturbations, Gamma, appears to be proportional to beta(2) and thus proportional to the square of the Brunt-Vaisala frequency (Gamma proportional to beta(2)proportional to N-2). The saturation level of Reynolds stresses, on the other hand, seems to be proportional to beta(1/2). This highlights the importance of baroclinic effects even for the low entropy gradients expected in protoplanetary disks.
C1 [Raettig, Natalie; Klahr, Hubert] Max Planck Inst Astron, D-69117 Heidelberg, Germany.
[Raettig, Natalie; Lyra, Wladimir] Amer Museum Nat Hist, Dept Astrophys, New York, NY 10024 USA.
[Lyra, Wladimir] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Raettig, N (reprint author), Max Planck Inst Astron, Konigstuhl 17, D-69117 Heidelberg, Germany.
EM raettig@mpia.de; Wladimir.Lyra@jpl.nasa.gov; klahr@mpia.de
FU National Institute for Computational Sciences (NICS) [TG-MCA99S024];
Annette Kade Graduate Student Fellowship Program at the American Museum
of Natural History
FX Our simulations were conducted partly on the MPIA cluster THEO in
Garching, and on the JUGENE machine of the JSC using the grand HHD19.
This work was partially supported by the National Institute for
Computational Sciences (NICS) under TG-MCA99S024 and utilized the NICS
Kraken system. This collaboration was made possible through the support
of the Annette Kade Graduate Student Fellowship Program at the American
Museum of Natural History. N.R. also thanks IMPRS-HD.
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SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD MAR 10
PY 2013
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AR 115
DI 10.1088/0004-637X/765/2/115
PG 12
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SC Astronomy & Astrophysics
GA 103MP
UT WOS:000315921500040
ER
PT J
AU Sorce, JG
Courtois, HM
Tully, RB
Seibert, M
Scowcroft, V
Freedman, WL
Madore, BF
Persson, SE
Monson, A
Rigby, J
AF Sorce, Jenny G.
Courtois, Helene M.
Tully, R. Brent
Seibert, Mark
Scowcroft, Victoria
Freedman, Wendy L.
Madore, Barry F.
Persson, S. Eric
Monson, Andy
Rigby, Jane
TI CALIBRATION OF THE MID-INFRARED TULLY-FISHER RELATION
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE cosmological parameters; distance scale; galaxies: clusters: general;
galaxies: distances and redshifts; galaxies: photometry; radio lines:
galaxies
ID SPITZER-SPACE-TELESCOPE; CARNEGIE HUBBLE PROGRAM; INFRARED ARRAY CAMERA;
4.5 MU-M; ENERGY-DISTRIBUTIONS; LUMINOSITY FUNCTION; CLUSTER GALAXIES;
NEARBY GALAXIES; SPIRAL GALAXIES; DISTANCE
AB Distance measures on a coherent scale around the sky are required to address the outstanding cosmological problems of the Hubble constant and of departures from the mean cosmic flow. The correlation between galaxy luminosities and rotation rates can be used to determine the distances to many thousands of galaxies in a wide range of environments potentially out to 200 Mpc. Mid-infrared (3.6 mu m) photometry with the Spitzer Space Telescope is particularly valuable as a source of luminosities because it provides products of uniform quality across the sky. From a perch above the atmosphere, essentially the total magnitude of targets can be registered in exposures of a few minutes. Extinction is minimal and the flux is dominated by the light from old stars, which is expected to correlate with the mass of the targets.
In spite of the superior photometry, the correlation between mid-infrared luminosities and rotation rates extracted from neutral hydrogen profiles is slightly degraded from the correlation found with I-band luminosities. A color correction recovers a correlation that provides comparable accuracy to that available at the I band (similar to 20% 1 sigma in an individual distance) while retaining the advantages identified above. Without color correction, the relation between linewidth and [3.6] magnitudes is M-[3.6](b,i,k,a) = -20.34 - 9.74(log(mx)(Wi) - 2.5). This description is found with a sample of 213 galaxies in 13 clusters that define the slope and 26 galaxies with Cepheid or tip of the red giant branch distances that define the zero point. A color-corrected parameter M-C[3.6] is constructed that has reduced scatter: M-C[3.6] = -20.34 - 9.13(log(mx)(Wi) - 2.5). Consideration of the seven calibration clusters beyond 50 Mpc, outside the domain of obvious peculiar velocities, provides a preliminary Hubble constant estimate of H-0 = 74 +/- 4 km s(-1) Mpc(-1).
C1 [Sorce, Jenny G.; Courtois, Helene M.] Univ Lyon 1, Inst Phys Nucl, F-69365 Lyon, France.
[Courtois, Helene M.; Tully, R. Brent] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA.
[Seibert, Mark; Scowcroft, Victoria; Freedman, Wendy L.; Madore, Barry F.; Persson, S. Eric; Monson, Andy] Carnegie Observ, Pasadena, CA 91101 USA.
[Rigby, Jane] NASA, Goddard Space Flight Ctr, Observat Cosmol Lab, Greenbelt, MD 20771 USA.
RP Sorce, JG (reprint author), Univ Lyon 1, Inst Phys Nucl, F-69365 Lyon, France.
EM j.sorce@ipnl.in2p3.fr
RI Rigby, Jane/D-4588-2012
OI Rigby, Jane/0000-0002-7627-6551
FU NASA through the Spitzer Science Center [61009, 80072]; US National
Science Foundation [AST-0908846]
FX The data used in this paper are available at the Extragalactic Distance
Database. 6 The photometric data are found by selecting the catalog
Spitzer [3.6]-Band Photometry and then a galaxy of choice, while the Hi
profiles are found in the catalog All Digital HI. We thank Tom Jarrett,
part of the Cosmic Flows with Spitzer collaboration, for advice on
Spitzer photometry and James Shombert for his development of Archangel.
Much of the data used here come from the Spitzer Space Telescope
archive. We thank Kartik Sheth for the contribution of his program
Spitzer Survey of Stellar Structure in Galaxies. NASA through the
Spitzer Science Center provides support for CHP, the Carnegie Hubble
Program, cycle 6 program 61009 and for CFS, Cosmic Flows with Spitzer,
cycle 8 program 80072. R.B.T. receives support from the US National
Science Foundation with award AST-0908846.
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD MAR 10
PY 2013
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SC Astronomy & Astrophysics
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UT WOS:000315921500019
ER
PT J
AU Teng, SH
Veilleux, S
Baker, AJ
AF Teng, Stacy H.
Veilleux, Sylvain
Baker, Andrew J.
TI GREEN BANK TELESCOPE DETECTION OF POLARIZATION-DEPENDENT HI ABSORPTION
AND HI OUTFLOWS IN LOCAL ULIRGs AND QUASARS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: active; galaxies: evolution; ISM: jets and outflows; quasars:
absorption lines; radio lines: galaxies
ID ULTRALUMINOUS INFRARED GALAXIES; ACTIVE GALACTIC NUCLEI; RADIO-QUIET
QUASARS; SCALE GASEOUS OUTFLOWS; II ESI SPECTRA; NEUTRAL HYDROGEN;
STAR-FORMATION; BLACK-HOLES; SPITZER QUASAR; HOST GALAXIES
AB We present the results of a 21 cm HI survey of 27 local massive gas-rich late-stage mergers and merger remnants with the Robert C. Byrd Green Bank Telescope. These remnants were selected from the Quasar/ULIRG Evolution Study sample of ultraluminous infrared galaxies (ULIRGs; L8-1000 mu m > 10(12) L-circle dot) and quasars; our targets are all bolometrically dominated by active galactic nuclei (AGNs) and sample the later phases of the proposed ULIRG-to-quasar evolutionary sequence. We find the prevalence of Hi absorption (emission) to be 100% (29%) in ULIRGs with HI detections, 100% (88%) in FIR-strong quasars, and 63% (100%) in FIR-weak quasars. The absorption features are associated with powerful neutral outflows that change from being mainly driven by star formation in ULIRGs to being driven by the AGN in the quasars. These outflows have velocities that exceed 1500 km s(-1) in some cases. Unexpectedly, we find polarization-dependent Hi absorption in 57% of our spectra (88% and 63% of the FIR-strong and FIR-weak quasars, respectively). We attribute this result to absorption of polarized continuum emission from these sources by foreground HI clouds. About 60% of the quasars displaying polarized spectra are radio-loud, far higher than the similar to 10% observed in the general AGN population. This discrepancy suggests that radio jets play an important role in shaping the environments in these galaxies. These systems may represent a transition phase in the evolution of gas-rich mergers into "mature" radio galaxies.
C1 [Teng, Stacy H.] NASA, Goddard Space Flight Ctr, Observat Cosmol Lab, Greenbelt, MD 20771 USA.
[Veilleux, Sylvain] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Veilleux, Sylvain] Univ Maryland, Joint Space Sci Inst, College Pk, MD 20742 USA.
[Veilleux, Sylvain] NASA, Goddard Space Flight Ctr, Astroparticle Phys Lab, Greenbelt, MD 20771 USA.
[Veilleux, Sylvain] Max Planck Inst Extraterr Phys, D-85741 Garching, Germany.
[Baker, Andrew J.] Rutgers State Univ, Dept Phys & Astron, Piscataway, NJ 08854 USA.
RP Teng, SH (reprint author), NASA, Postdoctoral Program, Greenbelt, MD 20771 USA.
EM stacy.h.teng@nasa.gov
FU NASA; NASA Postdoctoral Program (NPP) Fellowship; Senior NPP award;
Humboldt Foundation
FX We are grateful to the anonymous referee for providing useful comments
that improved the paper. We thank the GBT operators and the Green Bank
staff, especially Ron Maddalena, for support during this program
(11B-075, 12A-123), as well as Tim Robishaw and Lisa Wei for useful
discussions. We also thank Sheila Kannappan and her team for allowing us
to examine their proprietary data on PG 1501+106. The National Radio
Astronomy Observatory is a facility of the National Science Foundation
operated under cooperative agreement by Associated Universities, Inc. We
made use of the NASA/IPAC Extragalactic Databased (NED), which is
operated by the Jet Propulsion Laboratory, Caltech, under contract with
NASA. We also acknowledge the usage of the HyperLeda database
(http://leda.univ-lyon1.fr). S.H. T. is supported by a NASA Postdoctoral
Program (NPP) Fellowship. S. V. acknowledges support from a Senior NPP
award held at the NASA Goddard Space Flight Center and from the Humboldt
Foundation which provided funds for a long-term visit at MPE in 2012.
NR 79
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U1 0
U2 4
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD MAR 10
PY 2013
VL 765
IS 2
AR 95
DI 10.1088/0004-637X/765/2/95
PG 18
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 103MP
UT WOS:000315921500020
ER
PT J
AU Gopalswamy, N
Xie, H
Akiyama, S
Yashiro, S
Usoskin, IG
Davila, JM
AF Gopalswamy, N.
Xie, H.
Akiyama, S.
Yashiro, S.
Usoskin, I. G.
Davila, J. M.
TI THE FIRST GROUND LEVEL ENHANCEMENT EVENT OF SOLAR CYCLE 24: DIRECT
OBSERVATION OF SHOCK FORMATION AND PARTICLE RELEASE HEIGHTS
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE acceleration of particles; shock waves; Sun: coronal mass ejections
(CMEs); Sun: flares; Sun: particle emission; Sun: radio radiation
ID CORONAL MASS EJECTIONS; ENERGETIC PARTICLES
AB We report on the 2012 May 17 ground level enhancement (GLE) event, which is the first of its kind in solar cycle 24. This is the first GLE event to be fully observed close to the surface by the Solar Terrestrial Relations Observatory (STEREO) mission. We determine the coronal mass ejection (CME) height at the start of the associated metric type II radio burst (i.e., shock formation height) as 1.38 Rs (from the Sun center). The CME height at the time of GLE particle release was directly measured from a STEREO image as 2.32 Rs, which agrees well with the estimation from CME kinematics. These heights are consistent with those obtained for cycle-23 GLEs using back-extrapolation. By contrasting the 2012 May 17 GLE with six other non-GLE eruptions from well-connected regions with similar or larger flare sizes and CME speeds, we find that the latitudinal distance from the ecliptic is rather large for the non-GLE events due to a combination of non-radial CME motion and unfavorable solar B0 angle, making the connectivity to Earth poorer. We also find that the coronal environment may play a role in deciding the shock strength.
C1 [Gopalswamy, N.; Xie, H.; Akiyama, S.; Yashiro, S.; Davila, J. M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Xie, H.; Akiyama, S.; Yashiro, S.] Catholic Univ Amer, Washington, DC 20064 USA.
[Usoskin, I. G.] Univ Oulu, Sodankyla Geophys Observ, Oulu Unit, FI-90014 Oulu, Finland.
[Usoskin, I. G.] Univ Oulu, Dept Phys, FI-90014 Oulu, Finland.
RP Gopalswamy, N (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RI Usoskin, Ilya/E-5089-2014
OI Usoskin, Ilya/0000-0001-8227-9081
FU NASA/LWS program
FX STEREO is a mission in NASA's Solar Terrestrial Probes program. SOHO is
a project of international collaboration between ESA and NASA. Work
supported by NASA/LWS program. Oulu NM data are available at
http://cosmicrays.oulu.fi.
NR 16
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U1 0
U2 6
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 2041-8205
EI 2041-8213
J9 ASTROPHYS J LETT
JI Astrophys. J. Lett.
PD MAR 10
PY 2013
VL 765
IS 2
AR L30
DI 10.1088/2041-8205/765/2/L30
PG 5
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 097QR
UT WOS:000315489100006
ER
PT J
AU Koss, M
Mushotzky, R
Baumgartner, W
Veilleux, S
Tueller, J
Markwardt, C
Casey, CM
AF Koss, Michael
Mushotzky, Richard
Baumgartner, Wayne
Veilleux, Sylvain
Tueller, Jack
Markwardt, Craig
Casey, Caitlin M.
TI STUDYING FAINT ULTRA-HARD X-RAY EMISSION FROM AGN IN GOALS LIRGS WITH
SWIFT/BAT
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE galaxies: active; X-rays: galaxies
ID ACTIVE GALACTIC NUCLEUS; LUMINOUS INFRARED GALAXIES; CHANDRA;
DIAGNOSTICS; DISCOVERY; SAMPLE; QUEST; QSOS
AB We present the first analysis of the all-sky Swift Burst Alert Telescope (BAT) ultra-hard X-ray (14-195 keV) data for a targeted list of objects. We find that the BAT data can be studied at three-times-fainter limits than in previous blind detection catalogs based on prior knowledge of source positions and using smaller energy ranges for source detection. We determine the active galactic nucleus (AGN) fraction in 134 nearby (z < 0.05) luminous infrared galaxies (LIRGs) from the GOALS sample. We find that LIRGs have a higher detection frequency than galaxies matched in stellar mass and redshift at 14-195 keV and 24-35 keV. In agreement with work at other wavelengths, the AGN detection fraction increases strongly at high IR luminosity with half of the high-luminosity LIRGs (50%, 6/12, log L-IR/L-circle dot > 11.8) detected. The BAT AGN classification shows 97% (37/38) agreement with Chandra and XMM-Newton AGN classification using hardness ratios or detection of an iron K alpha line. This confirms our statistical analysis and supports the use of the Swift/BAT all-sky survey to study fainter populations of any category of sources in the ultra-hard X-ray band. BAT AGNs in LIRGs tend to show higher column densities with 40% +/- 9% showing 14-195 keV/2-10 keV hardness flux ratios suggestive of high or Compton-thick column densities (log N-H > 24 cm(-2)), compared to only 12% +/- 5% of non-LIRG BAT AGNs. We also find that using specific energy ranges of the BAT detector can yield additional sources over total band detections with 24% (5/21) of detections in LIRGs at 24-35 keV not detected at 14-195 keV.
C1 [Koss, Michael; Casey, Caitlin M.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA.
[Mushotzky, Richard; Veilleux, Sylvain] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Baumgartner, Wayne; Veilleux, Sylvain; Tueller, Jack; Markwardt, Craig] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA.
RP Koss, M (reprint author), Univ Hawaii, Inst Astron, 2680 Woodlawn Dr, Honolulu, HI 96822 USA.
EM koss@ifa.hawaii.edu
RI Koss, Michael/B-1585-2015;
OI Koss, Michael/0000-0002-7998-9581; Casey, Caitlin/0000-0002-0930-6466
NR 26
TC 20
Z9 20
U1 0
U2 3
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 2041-8205
J9 ASTROPHYS J LETT
JI Astrophys. J. Lett.
PD MAR 10
PY 2013
VL 765
IS 2
AR L26
DI 10.1088/2041-8205/765/2/L26
PG 6
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 097QR
UT WOS:000315489100002
ER
PT J
AU LaMassa, SM
Heckman, TM
Ptak, A
Urry, CM
AF LaMassa, Stephanie M.
Heckman, T. M.
Ptak, A.
Urry, C. Megan
TI ON THE STAR FORMATION-AGN CONNECTION AT z less than or similar to 0.3
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE galaxies: active; galaxies: Seyfert; galaxies: star formation
ID DIGITAL SKY SURVEY; ACTIVE GALACTIC NUCLEI; SUPERMASSIVE BLACK-HOLES;
GALAXY MERGERS; VELOCITY DISPERSION; STARBURST GALAXIES; REDSHIFT
GALAXIES; DATA RELEASE; QUASARS; EVOLUTION
AB Using the spectra of a sample of similar to 28,000 nearby obscured active galaxies from Data Release 7 of the Sloan Digital Sky Survey (SDSS), we probe the connection between active galactic nucleus (AGN) activity and star formation over a range of radial scales in the host galaxy. We use the extinction-corrected luminosity of the [OIII] 5007 angstrom line as a proxy of intrinsic AGN power and supermassive black hole (SMBH) accretion rate. The star formation rates (SFRs) are taken from the MPA-JHU value-added catalog and are measured through the 3 '' SDSS aperture. We construct matched samples of galaxies covering a range in redshifts. With increasing redshift, the projected aperture size encompasses increasing amounts of the host galaxy. This allows us to trace the radial distribution of star formation as a function of AGN luminosity. We find that the star formation becomes more centrally concentrated with increasing AGN luminosity and Eddington ratio. This implies that such circumnuclear star formation is associated with AGN activity, and that it increasingly dominates over omnipresent disk star formation at higher AGN luminosities, placing critical constraints on theoretical models that link host galaxy star formation and SMBH fueling. We parameterize this relationship and find that the star formation on radial scales <1.7 kpc, when including a constant disk component, has a sub-linear dependence on SMBH accretion rate: SFR proportional to (M)over dot(0.36), suggesting that angular momentum transfer through the disk limits accretion efficiency rather than the supply from stellar mass loss.
C1 [LaMassa, Stephanie M.; Urry, C. Megan] Yale Univ, Dept Phys, Yale Ctr Astron Astrophys, New Haven, CT 06520 USA.
[Heckman, T. M.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA.
[Ptak, A.] NASA, GSFC, Greenbelt, MD 20770 USA.
RP LaMassa, SM (reprint author), Yale Univ, Dept Phys, Yale Ctr Astron Astrophys, POB 208121, New Haven, CT 06520 USA.
RI Urry, Claudia/G-7381-2011
OI Urry, Claudia/0000-0002-0745-9792
FU Alfred P. Sloan Foundation; National Science Foundation; U.S. Department
of Energy; National Aeronautics and Space Administration; Japanese
Monbukagakusho; Max Planck Society; Higher Education Funding Council for
England
FX We thank the referee for a careful reading of this manuscript. Funding
for the SDSS and SDSS-II has been provided by the Alfred P. Sloan
Foundation, the Participating Institutions, the National Science
Foundation, the U.S. Department of Energy, the National Aeronautics and
Space Administration, the Japanese Monbukagakusho, the Max Planck
Society, and the Higher Education Funding Council for England.
NR 44
TC 20
Z9 20
U1 0
U2 5
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 2041-8205
J9 ASTROPHYS J LETT
JI Astrophys. J. Lett.
PD MAR 10
PY 2013
VL 765
IS 2
AR L33
DI 10.1088/2041-8205/765/2/L33
PG 6
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 097QR
UT WOS:000315489100009
ER
PT J
AU McDonald, M
Benson, B
Veilleux, S
Bautz, MW
Reichardt, CL
AF McDonald, Michael
Benson, Bradford
Veilleux, Sylvain
Bautz, Marshall W.
Reichardt, Christian L.
TI AN HST/WFC3-UVIS VIEW OF THE STARBURST IN THE COOL CORE OF THE PHOENIX
CLUSTER
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE galaxies: active; galaxies: clusters: general; galaxies: clusters:
individual (SPT-CLJ2344-4243, Phoenix); galaxies: elliptical and
lenticular, cD; galaxies: starburst
ID ULTRALUMINOUS INFRARED GALAXIES; COLD MOLECULAR GAS; STAR-FORMATION;
FLOW CLUSTERS; ABELL 2597; SAMPLE; SPECTROSCOPY; EMISSION; A1795;
FILAMENTS
AB We present Hubble Space Telescope Wide Field Camera 3 observations of the core of the Phoenix cluster (SPT-CLJ2344-4243) in five broadband filters spanning rest-frame 1000-5500 angstrom. These observations reveal complex, filamentary blue emission, extending for >40 kpc from the brightest cluster galaxy. We observe an underlying, diffuse population of old stars, following an r(1/4) distribution, confirming that this system is somewhat relaxed. The spectral energy distribution in the inner part of the galaxy, as well as along the extended filaments, is a smooth continuum and is consistent with that of a star-forming galaxy, suggesting that the extended, filamentary emission is not due to the central active galactic nucleus, either from a large-scale ionized outflow or scattered polarized UV emission, but rather a massive population of young stars. We estimate an extinction-corrected star formation rate of 798 +/- 42 M-circle dot yr(-1), consistent with our earlier work based on low spatial resolution ultraviolet, optical, and infrared imaging. The lack of tidal features and multiple bulges, combine with the need for an exceptionally massive (>10(11) M-circle dot) cold gas reservoir, suggest that this star formation is not the result of a merger of gas-rich galaxies. Instead, we propose that the high X-ray cooling rate of similar to 2700 M-circle dot yr(-1) is the origin of the cold gas reservoir. The combination of such a high cooling rate and the relatively weak radio source in the cluster core suggests that feedback has been unable to halt cooling in this system, leading to this tremendous burst of star formation.
C1 [McDonald, Michael; Bautz, Marshall W.] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA.
[Benson, Bradford] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA.
[Veilleux, Sylvain] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Veilleux, Sylvain] Univ Maryland, Joint Space Sci Inst, College Pk, MD 20742 USA.
[Veilleux, Sylvain] NASA, Goddard Space Flight Ctr, Astroparticle Phys Lab, Greenbelt, MD 20771 USA.
[Veilleux, Sylvain] Max Planck Inst Extraterr Phys, D-85741 Garching, Germany.
[Reichardt, Christian L.] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA.
RP McDonald, M (reprint author), MIT, Kavli Inst Astrophys & Space Res, 77 Massachusetts Ave, Cambridge, MA 02139 USA.
EM mcdonald@space.mit.edu
OI Reichardt, Christian/0000-0003-2226-9169
FU NASA through STScI; NASA-GSFC; Humboldt Foundation; National Science
Foundation [ANT-0638937, PHY-1125897]; Kavli Foundation; CXC [13800883]
FX We thank the HST Director for graciously providing the data for this
program. M.M. acknowledges support provided by NASA through a Hubble
Fellowship grant from STScI. S.V. acknowledges support from a Senior NPP
Award held at NASA-GSFC and from the Humboldt Foundation to fund a
long-term visit at MPE in 2012. B.A.B. is supported by the National
Science Foundation through grant ANT-0638937, with partial support
provided by NSF grant PHY-1125897, the Kavli Foundation, and Chandra
Award Number 13800883 issued by the CXC.
NR 44
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U1 0
U2 3
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 2041-8205
J9 ASTROPHYS J LETT
JI Astrophys. J. Lett.
PD MAR 10
PY 2013
VL 765
IS 2
AR L37
DI 10.1088/2041-8205/765/2/L37
PG 6
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 097QR
UT WOS:000315489100013
ER
PT J
AU Stello, D
Huber, D
Bedding, TR
Benomar, O
Bildsten, L
Elsworth, YP
Gilliland, RL
Mosser, B
Paxton, B
White, TR
AF Stello, Dennis
Huber, Daniel
Bedding, Timothy R.
Benomar, Othman
Bildsten, Lars
Elsworth, Yvonne P.
Gilliland, Ronald L.
Mosser, Benoit
Paxton, Bill
White, Timothy R.
TI ASTEROSEISMIC CLASSIFICATION OF STELLAR POPULATIONS AMONG 13,000 RED
GIANTS OBSERVED BY KEPLER
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE asteroseismology; stars: evolution; stars: fundamental parameters;
stars: interiors; stars: oscillations; techniques: photometric
ID SOLAR-LIKE OSCILLATIONS; OPEN CLUSTERS; MIXED-MODES; NGC 6791; STARS;
ROTATION; SCIENCE; COROT
AB Of the more than 150,000 targets followed by the Kepler Mission, about 10% were selected as red giants. Due to their high scientific value, in particular for Galaxy population studies and stellar structure and evolution, their Kepler light curves were made public in late 2011. More than 13,000 (over 85%) of these stars show intrinsic flux variability caused by solar-like oscillations making them ideal for large-scale asteroseismic investigations. We automatically extracted individual frequencies and measured the period spacings of the dipole modes in nearly every red giant. These measurements naturally classify the stars into various populations, such as the red giant branch, the low-mass (M/M-circle dot less than or similar to 1.8) helium-core-burning red clump, and the higher-mass (M/M-circle dot greater than or similar to 1.8) secondary clump. The period spacings also reveal that a large fraction of the stars show rotationally induced frequency splittings. This sample of stars will undoubtedly provide an extremely valuable source for studying the stellar population in the direction of the Kepler field, in particular when combined with complementary spectroscopic surveys.
C1 [Stello, Dennis; Bedding, Timothy R.; Benomar, Othman; White, Timothy R.] Univ Sydney, Sch Phys, Sydney Inst Astron SIfA, Sydney, NSW 2006, Australia.
[Stello, Dennis; Bedding, Timothy R.; Benomar, Othman; White, Timothy R.] Aarhus Univ, Dept Phys & Astron, Stellar Astrophys Ctr, DK-8000 Aarhus C, Denmark.
[Huber, Daniel] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Bildsten, Lars; Paxton, Bill] Univ Calif Santa Barbara, Kavli Inst Theoret Phys, Santa Barbara, CA 93106 USA.
[Bildsten, Lars] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA.
[Elsworth, Yvonne P.] Univ Birmingham, Sch Phys & Astron, Birmingham B15 2TT, W Midlands, England.
[Gilliland, Ronald L.] Penn State Univ, Ctr Exoplanets & Habitable Worlds, University Pk, PA 16802 USA.
[Mosser, Benoit] Univ Paris 07, Observ Paris, Univ Paris 06, LESIA,CNRS, F-92195 Meudon, France.
RP Stello, D (reprint author), Univ Sydney, Sch Phys, Sydney Inst Astron SIfA, Sydney, NSW 2006, Australia.
OI Bedding, Timothy/0000-0001-5943-1460; Bedding, Tim/0000-0001-5222-4661
FU NASA's Science Mission Directorate; Australian Research Council
FX Funding for this Discovery mission is provided by NASA's Science Mission
Directorate. We thank the entire Kepler team without whom this
investigation would not have been possible. This research has been
supported by the Australian Research Council. D.H. is supported by an
appointment to the NASA Postdoctoral Program at Ames Research Center,
administered by Oak Ridge Associated Universities through a contract
with NASA.
NR 36
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U1 0
U2 2
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PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 2041-8205
EI 2041-8213
J9 ASTROPHYS J LETT
JI Astrophys. J. Lett.
PD MAR 10
PY 2013
VL 765
IS 2
AR L41
DI 10.1088/2041-8205/765/2/L41
PG 5
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 097QR
UT WOS:000315489100017
ER
PT J
AU Tiscareno, MS
Hedman, MM
Burns, JA
Castillo-Rogez, J
AF Tiscareno, Matthew S.
Hedman, Matthew M.
Burns, Joseph A.
Castillo-Rogez, Julie
TI COMPOSITIONS AND ORIGINS OF OUTER PLANET SYSTEMS: INSIGHTS FROM THE
ROCHE CRITICAL DENSITY
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE planets and satellites: composition; planets and satellites: dynamical
evolution and stability; planets and satellites: formation; planets and
satellites: rings
ID ORBITAL RESONANCES; SATELLITES; LARISSA; PROTEUS
AB We consider the Roche critical density (rho(Roche)), the minimum density of an orbiting object that, at a given distance from its planet, is able to hold itself together by self-gravity. It is directly related to the more familiar "Roche limit," the distance from a planet at which a strengthless orbiting object of given density is pulled apart by tides. The presence of a substantial ring requires that transient clumps have an internal density less than rho(Roche). Conversely, in the presence of abundant material for accretion, an orbiting object with density greater than rho(Roche) will grow. Comparing the rho(Roche) values at which the Saturn and Uranus systems transition rapidly from disruption-dominated (rings) to accretion-dominated (moons), we infer that the material composing Uranus' rings is likely more rocky, as well as less porous, than that composing Saturn's rings. From the high values of rho(Roche) at the innermost ring moons of Jupiter and Neptune, we infer that those moons may be composed of denser material than expected, or more likely that they are interlopers that formed farther from their planets and have since migrated inward, now being held together by internal material strength. Finally, the "Portia group" of eight closely packed Uranian moons has an overall surface density similar to that of Saturn's A ring. Thus, it can be seen as an accretion-dominated ring system, of similar character to the standard ring systems except that its material has a characteristic density greater than the local rho(Roche).
C1 [Tiscareno, Matthew S.; Hedman, Matthew M.] Cornell Univ, Ctr Radiophys & Space Res, Ithaca, NY 14853 USA.
[Burns, Joseph A.] Cornell Univ, Dept Astron, Ithaca, NY 14853 USA.
[Burns, Joseph A.] Cornell Univ, Coll Engn, Ithaca, NY 14853 USA.
[Castillo-Rogez, Julie] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Tiscareno, MS (reprint author), Cornell Univ, Ctr Radiophys & Space Res, Ithaca, NY 14853 USA.
FU NASA [NNX10AP94G]
FX We thank John Weiss, Doug Hamilton, Matija Cuk, and Rick Greenberg for
helpful conversations. M.S.T. acknowledges funding from the NASA Outer
Planets Research program (NNX10AP94G).
NR 22
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U1 0
U2 9
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 2041-8205
J9 ASTROPHYS J LETT
JI Astrophys. J. Lett.
PD MAR 10
PY 2013
VL 765
IS 2
AR L28
DI 10.1088/2041-8205/765/2/L28
PG 5
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 097QR
UT WOS:000315489100004
ER
PT J
AU Raatikainen, T
Nenes, A
Seinfeld, JH
Morales, R
Moore, RH
Lathem, TL
Lance, S
Padro, LT
Lin, JJ
Cerully, KM
Bougiatioti, A
Cozic, J
Ruehl, CR
Chuang, PY
Anderson, BE
Flagan, RC
Jonsson, H
Mihalopoulos, N
Smith, JN
AF Raatikainen, Tomi
Nenes, Athanasios
Seinfeld, John H.
Morales, Ricardo
Moore, Richard H.
Lathem, Terry L.
Lance, Sara
Padro, Luz T.
Lin, Jack J.
Cerully, Kate M.
Bougiatioti, Aikaterini
Cozic, Julie
Ruehl, Christopher R.
Chuang, Patrick Y.
Anderson, Bruce E.
Flagan, Richard C.
Jonsson, Haflidi
Mihalopoulos, Nikos
Smith, James N.
TI Worldwide data sets constrain the water vapor uptake coefficient in
cloud formation
SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF
AMERICA
LA English
DT Article
DE global climate; hydrological cycle; precipitation
ID DROPLET GROWTH-KINETICS; SIZE-RESOLVED CCN; ACTIVATION KINETICS; CLIMATE
MODELS; AEROSOL; HYGROSCOPICITY; CONDENSATION; GASES; ENVIRONMENT;
EMISSIONS
AB Cloud droplet formation depends on the condensation of water vapor on ambient aerosols, the rate of which is strongly affected by the kinetics of water uptake as expressed by the condensation (or mass accommodation) coefficient, alpha(c). Estimates of alpha(c) for droplet growth from activation of ambient particles vary considerably and represent a critical source of uncertainty in estimates of global cloud droplet distributions and the aerosol indirect forcing of climate. We present an analysis of 10 globally relevant data sets of cloud condensation nuclei to constrain the value of alpha(c) for ambient aerosol. We find that rapid activation kinetics (alpha(c) > 0.1) is uniformly prevalent. This finding resolves a long-standing issue in cloud physics, as the uncertainty in water vapor accommodation on droplets is considerably less than previously thought.
C1 [Raatikainen, Tomi; Nenes, Athanasios; Morales, Ricardo; Moore, Richard H.; Lathem, Terry L.; Lance, Sara; Padro, Luz T.; Lin, Jack J.; Cerully, Kate M.; Bougiatioti, Aikaterini] Georgia Inst Technol, Atlanta, GA 30332 USA.
[Raatikainen, Tomi] Finnish Meteorol Inst, FI-00101 Helsinki, Finland.
[Nenes, Athanasios; Mihalopoulos, Nikos] Fdn Res & Technol Hellas, Inst Chem Engn & High Temp Chem Proc, Patras 71110, Greece.
[Seinfeld, John H.; Moore, Richard H.; Flagan, Richard C.] CALTECH, Pasadenda, CA 91106 USA.
[Moore, Richard H.; Anderson, Bruce E.] NASA, Langley Res Ctr, Hampton, VA 23681 USA.
[Lance, Sara; Smith, James N.] Natl Ctr Atmospher Res, Atmospher Chem Div, Boulder, CO 80305 USA.
[Lance, Sara] SPEC Inc, Boulder, CO 80301 USA.
[Padro, Luz T.] Tufts Univ, Medford, MA 02155 USA.
[Bougiatioti, Aikaterini; Mihalopoulos, Nikos] Univ Crete, Dept Chem, Iraklion 71003, Greece.
[Cozic, Julie] NOAA, Div Chem Sci, Earth Syst Res Lab, Boulder, CO 80305 USA.
[Cozic, Julie] Lab Glaciol & Geophys Environm, F-38402 St Martin Dheres, France.
[Ruehl, Christopher R.] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Berkeley, CA 94720 USA.
[Chuang, Patrick Y.] Univ Calif Santa Cruz, Santa Cruz, CA 95064 USA.
[Jonsson, Haflidi] USN, Postgrad Sch, Monterey, CA 93943 USA.
[Smith, James N.] Univ Eastern Finland, Dept Appl Phys, Kuopio 70210, Finland.
RP Nenes, A (reprint author), Georgia Inst Technol, Atlanta, GA 30332 USA.
EM athanasios.nenes@gatech.edu
RI Smith, James/C-5614-2008; Moore, Richard/E-9653-2010; Raatikainen,
Tomi/C-5410-2014; Morales Betancourt, Ricardo/A-3827-2016; Mihalopoulos,
Nikolaos/H-5327-2016
OI Smith, James/0000-0003-4677-8224; Morales Betancourt,
Ricardo/0000-0002-5475-8605; Mihalopoulos, Nikolaos/0000-0002-1282-0896
FU Georgia Tech President's fellowship; National Center for Atmospheric
Research Advanced Study Program Graduate Fellowship; NASA Graduate
Student Researchers Program; Department of Energy Global Change
Education Fellowship; NASA Earth and Space Science Fellowship; NASA
postdoctoral fellowship; NASA Earth System Science fellowship; National
Science Foundation (NSF) fellowship; Georgia Tech institutional
fellowship; DOE grant; Electric Power Research Institute; NSF Faculty
Early Career Development award; NOAA grants; NASA grants
FX We thank Dr. Xiaohong Liu for advice on using the CAM 5.1 and for
providing computer time for the simulations. We also thank all those who
contributed to the measurement campaigns; Charles Brock from the
National Oceanic and Atmospheric Administration (NOAA) Earth System
Research Laboratory; and the National Aeronautics and Space
Administration (NASA) Langley Aerosol Research Group Experiment for
supporting aerosol measurements during Arctic Research of the
Composition of the Troposphere from Aircraft and Satellites. T. R.
thanks the Finnish Cultural Foundation; S. L. and J.J.L. acknowledge the
support of a Georgia Tech President's fellowship and an National Center
for Atmospheric Research Advanced Study Program Graduate Fellowship; and
J.J.L. thanks the NASA Graduate Student Researchers Program for funding.
R. H. M. acknowledges support from a Department of Energy Global Change
Education Fellowship, a NASA Earth and Space Science Fellowship, and a
NASA postdoctoral fellowship. L. T. P. received funding from a NASA
Earth System Science fellowship. T. L. L. acknowledges support from a
National Science Foundation (NSF) fellowship and a Georgia Tech
institutional fellowship. Funding from a DOE grant (to A.N.), the
Electric Power Research Institute, an NSF Faculty Early Career
Development award (to A.N.), NOAA grants (to J.H.S. and A.N.), and NASA
grants (to A.N.) is acknowledged.
NR 34
TC 16
Z9 16
U1 1
U2 52
PU NATL ACAD SCIENCES
PI WASHINGTON
PA 2101 CONSTITUTION AVE NW, WASHINGTON, DC 20418 USA
SN 0027-8424
J9 P NATL ACAD SCI USA
JI Proc. Natl. Acad. Sci. U. S. A.
PD MAR 5
PY 2013
VL 110
IS 10
BP 3760
EP 3764
DI 10.1073/pnas.1219591110
PG 5
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 109OH
UT WOS:000316377400030
PM 23431189
ER
PT J
AU Kozorezov, AG
Lambert, CJ
Bandler, SR
Balvin, MA
Busch, SE
Nagler, PN
Porst, JP
Smith, SJ
Stevenson, TR
Sadleir, JE
AF Kozorezov, Alexander G.
Lambert, Colin J.
Bandler, Simon R.
Balvin, Manuel A.
Busch, Sarah E.
Nagler, Peter N.
Porst, Jan-Patrick
Smith, Stephen J.
Stevenson, Thomas R.
Sadleir, John E.
TI Athermal energy loss from x-rays deposited in thin superconducting films
on solid substrates
SO PHYSICAL REVIEW B
LA English
DT Article
ID TRANSITION-EDGE SENSORS; TUNNEL-JUNCTIONS; MAGNETIC CALORIMETERS;
RESOLUTION; PERFORMANCE; DETECTORS; METALS; MICROCALORIMETERS;
SPECTROSCOPY; SCATTERING
AB When energy is deposited in a thin-film cryogenic detector, such as from the absorption of an x-ray, an important feature that determines the energy resolution is the amount of athermal energy that can be lost to the heat bath prior to the elementary excitation systems coming into thermal equilibrium. This form of energy loss will be position dependent and therefore can limit the detector energy resolution. An understanding of the physical processes that occur when elementary excitations are generated in metal films on dielectric substrates is important for the design and optimization of a number of different types of low-temperature detectors. We have measured the total energy loss in one relatively simple geometry that allows us to study these processes and compare measurements with calculation based upon a model for the various different processes. We have modeled the athermal phonon energy loss in this device by finding an evolving phonon distribution function that solves the system of kinetic equations for the interacting system of electrons and phonons. Using measurements of device parameters such as the Debye energy and the thermal diffusivity we have calculated the expected energy loss from this detector geometry, and also the position-dependent variation of this loss. We have also calculated the predicted impact on measured spectral lineshapes and have shown that they agree well with measurements. In addition, we have tested this model by using it to predict the performance of a number of other types of detector with different geometries, where good agreement is also found. DOI: 10.1103/PhysRevB.87.104504
C1 [Kozorezov, Alexander G.; Lambert, Colin J.] Univ Lancaster, Dept Phys, Lancaster, England.
[Bandler, Simon R.; Balvin, Manuel A.; Busch, Sarah E.; Nagler, Peter N.; Porst, Jan-Patrick; Smith, Stephen J.; Stevenson, Thomas R.; Sadleir, John E.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Nagler, Peter N.; Porst, Jan-Patrick] Brown Univ, Dept Phys, Providence, RI 02912 USA.
RP Kozorezov, AG (reprint author), Univ Lancaster, Dept Phys, Lancaster, England.
RI Smith, Stephen/B-1256-2008; Bandler, Simon/A-6258-2010
OI Smith, Stephen/0000-0003-4096-4675; Bandler, Simon/0000-0002-5112-8106
NR 43
TC 10
Z9 10
U1 0
U2 23
PU AMER PHYSICAL SOC
PI COLLEGE PK
PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA
SN 2469-9950
EI 2469-9969
J9 PHYS REV B
JI Phys. Rev. B
PD MAR 5
PY 2013
VL 87
IS 10
AR 104504
DI 10.1103/PhysRevB.87.104504
PG 15
WC Physics, Condensed Matter
SC Physics
GA 100US
UT WOS:000315730200003
ER
PT J
AU Asthana, R
Singh, M
Martinez-Fernandez, J
AF Asthana, R.
Singh, M.
Martinez-Fernandez, J.
TI Joining and interface characterization of in situ reinforced silicon
nitride
SO JOURNAL OF ALLOYS AND COMPOUNDS
LA English
DT Article
DE Ceramics; Thermal expansion; Transmission electron microscopy; Nitride
materials; Surfaces and interfaces
ID DIFFRACTION PATTERNS; FILLER ALLOYS; CU; MICROSTRUCTURE; JOINTS;
CERAMICS; STRENGTH; PHASES; SI3N4; STEEL
AB Copper-base active metal interlayers were used to bond in situ reinforced silicon nitride (Honeywell AS800) at 1317 K for 5 and 30 min in vacuum. The joints were characterized using scanning electron microscopy (SEM), energy dispersive spectroscopy (EDS), electron back scattered diffraction (EBSD), and transmission electron microscopy (TEM). A Ti-rich interaction zone (similar to 3.0-3.5 mu m thick) formed at the Si3N4/braze interface. This reaction layer grew toward the inner part of the joint with a featureless microstructure, creating a strong bond. Regions of a Ti-rich phase were frequently found next to the reaction layer but surrounded by the Cu alloy. Extensive Ti and Si enrichments were noted at the interface but there was no evidence of interfacial segregation of Y, La, and Sr (from Y2O3, La2O3 and SrO, added as sintering aids). The reaction layer thickness and composition did not change when brazing time increased from 5 min to 30 min suggesting rapid growth kinetics in the early stages of reaction. The joints were crack-free and showed features associated with plastic deformation, which indicated that the metal interlayer accommodated strain associated with CTE mismatch. The inner part of the joint consisted of highly textured large grains of the braze alloy. (C) 2012 Elsevier B. V. All rights reserved.
C1 [Asthana, R.] Univ Wisconsin Stout, Dept Engn & Technol, Menomonie, WI 54751 USA.
[Singh, M.] NASA, Ohio Aerosp Inst, Glenn Res Ctr, Cleveland, OH 44135 USA.
[Martinez-Fernandez, J.] Univ Seville, CSIC, Dpto Fis Mat Condensada, ICMSE, E-41012 Seville, Spain.
RP Asthana, R (reprint author), Univ Wisconsin Stout, Dept Engn & Technol, 326 FH, Menomonie, WI 54751 USA.
EM asthanar@uwstout.edu; Mrityunjay.Singh@nasa.gov; Martinez@us.es
RI MARTINEZ FERNANDEZ, JULIAN/K-1826-2012
OI MARTINEZ FERNANDEZ, JULIAN/0000-0002-1199-6638
FU NASA Glenn Research Center
FX Rajiv Asthana and Julian Martinez-Fernandez acknowledge the support
received from the NASA Glenn Research Center. Thanks are due F.M. Varela
and J. Ramirez-Rico, for their help with EBSD, SEM and TEM work, which
was performed at CITIUS (University of Sevilla).
NR 30
TC 4
Z9 4
U1 1
U2 69
PU ELSEVIER SCIENCE SA
PI LAUSANNE
PA PO BOX 564, 1001 LAUSANNE, SWITZERLAND
SN 0925-8388
J9 J ALLOY COMPD
JI J. Alloy. Compd.
PD MAR 5
PY 2013
VL 552
BP 137
EP 145
DI 10.1016/j.jallcom.2012.09.104
PG 9
WC Chemistry, Physical; Materials Science, Multidisciplinary; Metallurgy &
Metallurgical Engineering
SC Chemistry; Materials Science; Metallurgy & Metallurgical Engineering
GA 072EZ
UT WOS:000313653300024
ER
PT J
AU Roithmayr, CM
Hodges, DH
AF Roithmayr, Carlos M.
Hodges, Dewey H.
TI Identifying Sets of Constraint Forces by Inspection
SO JOURNAL OF APPLIED MECHANICS-TRANSACTIONS OF THE ASME
LA English
DT Article
DE holonomic constraint equations; nonholonomic constraint equations;
Lagrange multipliers; undetermined multipliers; Kane's method;
constraint forces
ID NATURAL ORTHOGONAL COMPLEMENT; SYSTEMS; MOTION; FORMULATION; EQUATIONS;
DYNAMICS
AB A mechanical system is often modeled as a set of particles and rigid bodies, some of which are constrained in one way or another. A concise method is proposed for identifying a set of constraint forces needed to ensure the restrictions are met. Identification consists of determining the direction of each constraint force and the point at which it must be applied, as well as the direction of the torque of each constraint force couple, together with the body on which the couple acts. This important information can be determined simply by inspecting constraint equations written in vector form. For the kinds of constraints commonly encountered, the constraint equations are expressed in terms of dot products involving velocities of the affected points or particles and angular velocities of the bodies concerned. The technique of expressing constraint equations in vector form and identifying constraint forces by inspection is useful when one is deriving explicit, analytical equations of motion by hand or with the aid of symbolic algebra software, as demonstrated with several examples.
C1 [Roithmayr, Carlos M.] NASA, Langley Res Ctr, Hampton, VA 23681 USA.
[Hodges, Dewey H.] Georgia Inst Technol, Sch Aerosp Engn, Atlanta, GA 30332 USA.
RP Roithmayr, CM (reprint author), NASA, Langley Res Ctr, Hampton, VA 23681 USA.
EM carlos.m.roithmayr@nasa.gov; dhodges@gatech.edu
NR 20
TC 0
Z9 0
U1 1
U2 2
PU ASME
PI NEW YORK
PA TWO PARK AVE, NEW YORK, NY 10016-5990 USA
SN 0021-8936
EI 1528-9036
J9 J APPL MECH-T ASME
JI J. Appl. Mech.-Trans. ASME
PD MAR
PY 2013
VL 80
IS 2
AR 021019
DI 10.1115/1.4007577
PG 13
WC Mechanics
SC Mechanics
GA 241OB
UT WOS:000326175400032
ER
PT J
AU Coddington, O
Pilewskie, P
Schmidt, KS
McBride, PJ
Vukicevic, T
AF Coddington, Odele
Pilewskie, Peter
Schmidt, K. Sebastian
McBride, Patrick J.
Vukicevic, Tomislava
TI Characterizing a New Surface-Based Shortwave Cloud Retrieval Technique,
Based on Transmitted Radiance for Soil and Vegetated Surface Types
SO ATMOSPHERE
LA English
DT Article
DE radiation: transmission and scattering; remote sensing; clouds and
aerosols; Shannon information content
ID MICROPHYSICAL PROPERTY RETRIEVALS; OBJECTIVE ASSESSMENT;
INFORMATION-CONTENT; RADIATIVE-TRANSFER; OPTICAL-THICKNESS; GLOBAL
OCEANS; ALBEDO; REFLECTANCE; SCATTERING; ALGORITHM
AB This paper presents an approach using the GEneralized Nonlinear Retrieval Analysis (GENRA) tool and general inverse theory diagnostics including the maximum likelihood solution and the Shannon information content to investigate the performance of a new spectral technique for the retrieval of cloud optical properties from surface based transmittance measurements. The cumulative retrieval information over broad ranges in cloud optical thickness (tau), droplet effective radius (r(e)), and overhead sun angles is quantified under two conditions known to impact transmitted radiation; the variability in land surface albedo and atmospheric water vapor content. Our conclusions are: (1) the retrieved cloud properties are more sensitive to the natural variability in land surface albedo than to water vapor content; (2) the new spectral technique is more accurate (but still imprecise) than a standard approach, in particular for tau between 5 and 60 and r(e) less than approximately 20 mu m; and (3) the retrieved cloud properties are dependent on sun angle for clouds of tau from 5 to 10 and r(e) < 10 mu m, with maximum sensitivity obtained for an overhead sun.
C1 [Coddington, Odele; Pilewskie, Peter; Schmidt, K. Sebastian] Univ Colorado, Lab Atmospher & Space Phys, Boulder, CO 80305 USA.
[Pilewskie, Peter] Univ Colorado, Dept Atmospher & Ocean Sci, Boulder, CO 80309 USA.
[McBride, Patrick J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Vukicevic, Tomislava] NOAA, Atlantic Oceanog & Meteorol Lab, Miami, FL 33149 USA.
RP Coddington, O (reprint author), Univ Colorado, Lab Atmospher & Space Phys, 3665 Discovery Dr, Boulder, CO 80305 USA.
EM odele.coddington@lasp.colorado.edu; peter.pilewskie@lasp.colorado.edu;
sebastian.schmidt@lasp.colorado.edu; patrick.mcbride@nasa.gov;
tomislava.vukicevic@noaa.gov
RI Vukicevic, Tomislava/B-1386-2014; Coddington, Odele/F-6342-2012;
Richards, Amber/K-8203-2015; SCHMIDT, KONRAD SEBASTIAN/C-1258-2013
OI Coddington, Odele/0000-0002-4338-7028; SCHMIDT, KONRAD
SEBASTIAN/0000-0003-3899-228X
FU NASA [NNX08AI83G, NNX11AK67G]
FX We gratefully acknowledge Shi Song for assistance in compiling the
forward modeling results and Bruce Kindel for computing the linear
mixtures of soil and vegetated surface reflectance spectra. This work
was accomplished under NASA grant numbers NNX08AI83G and NNX11AK67G. We
would like to thank three anonymous reviewers for their helpful
comments, which improved this manuscript.
NR 37
TC 2
Z9 2
U1 1
U2 8
PU MDPI AG
PI BASEL
PA POSTFACH, CH-4005 BASEL, SWITZERLAND
SN 2073-4433
J9 ATMOSPHERE-BASEL
JI Atmosphere
PD MAR
PY 2013
VL 4
IS 1
BP 48
EP 71
DI 10.3390/atmos4010048
PG 24
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 175RH
UT WOS:000321249000004
ER
PT J
AU Kardashev, NS
Khartov, VV
Abramov, VV
Avdeev, VY
Alakoz, AV
Aleksandrov, YA
Ananthakrishnan, S
Andreyanov, VV
Andrianov, AS
Antonov, NM
Artyukhov, MI
Arkhipov, MY
Baan, W
Babakin, NG
Babyshkin, VE
Bartel', N
Belousov, KG
Belyaev, AA
Berulis, JJ
Burke, BF
Biryukov, AV
Bubnov, AE
Burgin, MS
Busca, G
Bykadorov, AA
Bychkova, VS
Vasil'kov, VI
Wellington, KJ
Vinogradov, IS
Wietfeldt, R
Voitsik, PA
Gvamichava, AS
Girin, IA
Gurvits, LI
Dagkesamanskii, RD
D'Addario, L
Giovannini, G
Jauncey, DL
Dewdney, PE
D'yakov, AA
Zharov, VE
Zhuravlev, VI
Zaslavskii, GS
Zakhvatkin, MV
Zinov'ev, AN
Ilinen, Y
Ipatov, AV
Kanevskii, BZ
Knorin, IA
Casse, JL
Kellermann, KI
Kovalev, YA
Kovalev, YY
Kovalenko, AV
Kogan, BL
Komaev, RV
Konovalenko, AA
Kopelyanskii, GD
Korneev, YA
Kostenko, VI
Kotik, AN
Kreisman, BB
Kukushkin, AY
Kulishenko, VF
Cooper, DN
Kut'kin, AM
Cannon, WH
Larionov, MG
Lisakov, MM
Litvinenko, LN
Likhachev, SF
Likhacheva, LN
Lobanov, AP
Logvinenko, SV
Langston, G
McCracken, K
Medvedev, SY
Melekhin, MV
Menderov, AV
Murphy, DW
Mizyakina, TA
Mozgovoi, YV
Nikolaev, NY
Novikov, BS
Novikov, ID
Oreshko, VV
Pavlenko, YK
Pashchenko, IN
Ponomarev, YN
Popov, MV
Pravin-Kumar, A
Preston, RA
Pyshnov, VN
Rakhimov, IA
Rozhkov, VM
Romney, JD
Rocha, P
Rudakov, VA
Raisanen, A
Sazankov, SV
Sakharov, BA
Semenov, SK
Serebrennikov, VA
Schilizzi, RT
Skulachev, DP
Slysh, VI
Smirnov, AI
Smith, JG
Soglasnov, VA
Sokolovskii, KV
Sondaar, LH
Stepan'yants, VA
Turygin, MS
Turygin, SY
Tuchin, AG
Urpo, S
Fedorchuk, SD
Finkel'shtein, AM
Fomalont, EB
Fejes, I
Fomina, AN
Khapin, YB
Tsarevskii, GS
Zensus, JA
Chuprikov, AA
Shatskaya, MV
Shapirovskaya, NY
Sheikhet, AI
Shirshakov, AE
Schmidt, A
Shnyreva, LA
Shpilevskii, VV
Ekers, RD
Yakimov, VE
AF Kardashev, N. S.
Khartov, V. V.
Abramov, V. V.
Avdeev, V. Yu.
Alakoz, A. V.
Aleksandrov, Yu. A.
Ananthakrishnan, S.
Andreyanov, V. V.
Andrianov, A. S.
Antonov, N. M.
Artyukhov, M. I.
Arkhipov, M. Yu.
Baan, W.
Babakin, N. G.
Babyshkin, V. E.
Bartel', N.
Belousov, K. G.
Belyaev, A. A.
Berulis, J. J.
Burke, B. F.
Biryukov, A. V.
Bubnov, A. E.
Burgin, M. S.
Busca, G.
Bykadorov, A. A.
Bychkova, V. S.
Vasil'kov, V. I.
Wellington, K. J.
Vinogradov, I. S.
Wietfeldt, R.
Voitsik, P. A.
Gvamichava, A. S.
Girin, I. A.
Gurvits, L. I.
Dagkesamanskii, R. D.
D'Addario, L.
Giovannini, G.
Jauncey, D. L.
Dewdney, P. E.
D'yakov, A. A.
Zharov, V. E.
Zhuravlev, V. I.
Zaslavskii, G. S.
Zakhvatkin, M. V.
Zinov'ev, A. N.
Ilinen, Yu.
Ipatov, A. V.
Kanevskii, B. Z.
Knorin, I. A.
Casse, J. L.
Kellermann, K. I.
Kovalev, Yu. A.
Kovalev, Yu. Yu.
Kovalenko, A. V.
Kogan, B. L.
Komaev, R. V.
Konovalenko, A. A.
Kopelyanskii, G. D.
Korneev, Yu. A.
Kostenko, V. I.
Kotik, A. N.
Kreisman, B. B.
Kukushkin, A. Yu.
Kulishenko, V. F.
Cooper, D. N.
Kut'kin, A. M.
Cannon, W. H.
Larionov, M. G.
Lisakov, M. M.
Litvinenko, L. N.
Likhachev, S. F.
Likhacheva, L. N.
Lobanov, A. P.
Logvinenko, S. V.
Langston, G.
McCracken, K.
Medvedev, S. Yu.
Melekhin, M. V.
Menderov, A. V.
Murphy, D. W.
Mizyakina, T. A.
Mozgovoi, Yu. V.
Nikolaev, N. Ya.
Novikov, B. S.
Novikov, I. D.
Oreshko, V. V.
Pavlenko, Yu. K.
Pashchenko, I. N.
Ponomarev, Yu. N.
Popov, M. V.
Pravin-Kumar, A.
Preston, R. A.
Pyshnov, V. N.
Rakhimov, I. A.
Rozhkov, V. M.
Romney, J. D.
Rocha, P.
Rudakov, V. A.
Raisanen, A.
Sazankov, S. V.
Sakharov, B. A.
Semenov, S. K.
Serebrennikov, V. A.
Schilizzi, R. T.
Skulachev, D. P.
Slysh, V. I.
Smirnov, A. I.
Smith, J. G.
Soglasnov, V. A.
Sokolovskii, K. V.
Sondaar, L. H.
Stepan'yants, V. A.
Turygin, M. S.
Turygin, S. Yu.
Tuchin, A. G.
Urpo, S.
Fedorchuk, S. D.
Finkel'shtein, A. M.
Fomalont, E. B.
Fejes, I.
Fomina, A. N.
Khapin, Yu. B.
Tsarevskii, G. S.
Zensus, J. A.
Chuprikov, A. A.
Shatskaya, M. V.
Shapirovskaya, N. Ya.
Sheikhet, A. I.
Shirshakov, A. E.
Schmidt, A.
Shnyreva, L. A.
Shpilevskii, V. V.
Ekers, R. D.
Yakimov, V. E.
TI "RadioAstron"-A Telescope with a Size of 300 000 km: Main Parameters and
First Observational Results
SO ASTRONOMY REPORTS
LA English
DT Article
ID BASE-LINE INTERFEROMETRY; RADIO-SOURCES; WATER MASER; ORION-KL; VLBI;
SCALE; GHZ; SPACECRAFT; SATELLITE; DISTANCE
AB The Russian Academy of Sciences and Federal Space Agency, together with the participation of many international organizations, worked toward the launch of the RadioAstron orbiting space observatory with its onboard 10-m reflector radio telescope from the Baikonur cosmodrome on July 18, 2011. Together with some of the largest ground-based radio telescopes and a set of stations for tracking, collecting, and reducing the data obtained, this space radio telescope forms a multi-antenna ground-space radio interferometer with extremely long baselines, making it possible for the first time to study various objects in the Universe with angular resolutions a million times better than is possible with the human eye. The project is targeted at systematic studies of compact radio-emitting sources and their dynamics. Objects to be studied include supermassive black holes, accretion disks, and relativistic jets in active galactic nuclei, stellar-mass black holes, neutron stars and hypothetical quark stars, regions of formation of stars and planetary systems in our and other galaxies, interplanetary and interstellar plasma, and the gravitational field of the Earth. The results of ground-based and inflight tests of the space radio telescope carried out in both autonomous and ground-space interferometric regimes are reported. The derived characteristics are in agreement with the main requirements of the project. The astrophysical science program has begun. DOI: 10.1134/S1063772913030025
C1 [Kardashev, N. S.; Avdeev, V. Yu.; Alakoz, A. V.; Aleksandrov, Yu. A.; Andreyanov, V. V.; Andrianov, A. S.; Antonov, N. M.; Arkhipov, M. Yu.; Babakin, N. G.; Belousov, K. G.; Berulis, J. J.; Biryukov, A. V.; Burgin, M. S.; Bychkova, V. S.; Vasil'kov, V. I.; Vinogradov, I. S.; Voitsik, P. A.; Gvamichava, A. S.; Girin, I. A.; Dagkesamanskii, R. D.; Zhuravlev, V. I.; Zinov'ev, A. N.; Kanevskii, B. Z.; Knorin, I. A.; Kovalev, Yu. A.; Kovalev, Yu. Yu.; Kovalenko, A. V.; Kopelyanskii, G. D.; Korneev, Yu. A.; Kostenko, V. I.; Kotik, A. N.; Kreisman, B. B.; Kut'kin, A. M.; Larionov, M. G.; Lisakov, M. M.; Likhachev, S. F.; Likhacheva, L. N.; Logvinenko, S. V.; Mizyakina, T. A.; Nikolaev, N. Ya.; Novikov, B. S.; Novikov, I. D.; Oreshko, V. V.; Pashchenko, I. N.; Ponomarev, Yu. N.; Popov, M. V.; Pyshnov, V. N.; Rudakov, V. A.; Sazankov, S. V.; Slysh, V. I.; Smirnov, A. I.; Soglasnov, V. A.; Sokolovskii, K. V.; Fedorchuk, S. D.; Tsarevskii, G. S.; Chuprikov, A. A.; Shatskaya, M. V.; Shapirovskaya, N. Ya.; Shnyreva, L. A.; Yakimov, V. E.] PN Lebedev Phys Inst, Astro Space Ctr, Moscow 117924, Russia.
[Khartov, V. V.; Artyukhov, M. I.; Babyshkin, V. E.; Bartel', N.; Komaev, R. V.; Melekhin, M. V.; Menderov, A. V.; Mozgovoi, Yu. V.; Semenov, S. K.; Serebrennikov, V. A.; Sheikhet, A. I.; Shirshakov, A. E.] Lavochkin Sci & Prod Assoc, Moscow 141400, Russia.
[Abramov, V. V.; Turygin, M. S.; Turygin, S. Yu.] Russian Acad Sci, Inst Radio Technol & Elect, Moscow, Russia.
[Ananthakrishnan, S.; Pravin-Kumar, A.] Tata Inst Fundamental Res, Pune, Maharashtra, India.
[Baan, W.; Sondaar, L. H.] Netherlands Inst Radio Astron ASTRON, NL-7990 AA Dwingeloo, Netherlands.
[Belyaev, A. A.; Medvedev, S. Yu.; Pavlenko, Yu. K.; Sakharov, B. A.] Vremya Ch Joint Stock Co, Nizhnii Novgorod 603105, Russia.
[Burke, B. F.] MIT, Cambridge, MA 02139 USA.
[Bubnov, A. E.; Kukushkin, A. Yu.; Novikov, B. S.; Skulachev, D. P.; Khapin, Yu. B.] Russian Acad Sci, Inst Space Res, Moscow V71, Russia.
[Busca, G.; Rocha, P.] Observ Neuchatel, Neuchatel, Switzerland.
[Bykadorov, A. A.] Salut 27 Private Joint Stock Co, Res & Prod Enterprise, Nizhnii Novgorod 603105, Russia.
[Wellington, K. J.; Jauncey, D. L.; Cooper, D. N.; McCracken, K.; Ekers, R. D.] CSIRO Div Radio Phys, Australia Telescope Natl Facil, Sydney, NSW, Australia.
[Wietfeldt, R.; D'Addario, L.; Murphy, D. W.; Preston, R. A.; Smith, J. G.] NASA Jet Prop Lab, Pasadena, CA 91011 USA.
[Gurvits, L. I.; Casse, J. L.] Joint Inst VLBI Europe, NL-7990 AA Dwingeloo, Netherlands.
[Gurvits, L. I.] Delft Univ Technol, Fac Aerosp Engn, NL-2629 HS Delft, Netherlands.
[Giovannini, G.] INAF Ist Radioastron Bologna, I-40129 Bologna, Italy.
[Giovannini, G.] Univ Bologna, Dipartimento Astron, I-40126 Bologna, Italy.
[Dewdney, P. E.] Univ Manchester, SKA Program Dev Off, Manchester M13 9PL, Lancs, England.
[D'yakov, A. A.; Ipatov, A. V.; Rakhimov, I. A.; Finkel'shtein, A. M.; Shpilevskii, V. V.] Russian Acad Sci, Inst Appl Astron, St Petersburg 196140, Russia.
[Zharov, V. E.; Sokolovskii, K. V.] Moscow MV Lomonosov State Univ, Sternberg Astron Inst, Moscow 119992, Russia.
[Zaslavskii, G. S.; Zakhvatkin, M. V.; Stepan'yants, V. A.; Tuchin, A. G.] Russian Acad Sci, MV Keldysh Appl Math Inst, Moscow 125047, Russia.
[Ilinen, Yu.] Ilinen Co, Helsinki, Finland.
[Kellermann, K. I.; Fomalont, E. B.] Natl Radio Astron Observ, Charlottesville, VA 22903 USA.
[Kovalev, Yu. Yu.; Lobanov, A. P.; Zensus, J. A.; Schmidt, A.] Max Planck Inst Radio Astron, D-53121 Bonn, Germany.
[Kogan, B. L.] Moscow Energy Inst, Moscow, Russia.
[Konovalenko, A. A.; Kulishenko, V. F.; Litvinenko, L. N.] Natl Acad Sci Ukraine, Radio Astron Inst, UA-61002 Kharkov, Ukraine.
[Bartel', N.; Cannon, W. H.] York Univ, Dept Phys & Astron, Toronto, ON M3J 1P3, Canada.
[Langston, G.] Natl Radio Astron Observ, Green Bank, WV 24944 USA.
[Rozhkov, V. M.] Raketno Kosmicheskie Sistemy, Moscow 111250, Russia.
[Romney, J. D.] Natl Radio Astron Observ, Socorro, NM 87801 USA.
[Raisanen, A.; Urpo, S.] Aalto Univ, Dept Radio Sci & Engn, FI-00076 Aalto, Finland.
[Schilizzi, R. T.] Univ Manchester, Jodrell Bank Ctr Astrophys, Manchester M13 9PL, Lancs, England.
[Fejes, I.] FOMI Satellite Geodet Obsevatory, Renc, Hungary.
[Fomina, A. N.] Private Joint Stock Co, Ekol & Radiosvyaz, Nizhnii Novgorod 603105, Russia.
RP Kardashev, NS (reprint author), PN Lebedev Phys Inst, Astro Space Ctr, Leninsky Prospect 53, Moscow 117924, Russia.
EM ykovalev@avunda.asc.rssi.ru
RI pyshnov, victor/N-1011-2015; Kovalev, Yuri/N-1053-2015; Kovalenko,
Anatoly/N-1591-2015; Dagkesamanskii, Rustam/N-2113-2015; Oreshko,
Vasily/N-2568-2015; Andrianov, Andrey/N-2638-2015; Larionov,
Mikhail/N-2668-2015; Logvinenko, Sergey/A-4551-2014; Burgin,
Mikhail/M-4162-2015; Kardashev, Nikolai/O-6441-2015; Zhuravlev,
Vladimir/M-6848-2015; Soglasnov, Vladimir/O-7615-2015; Lisakov,
Mikhail/M-6034-2013; Voytsik, Petr/M-6075-2013; Kovalev,
Yuri/J-5671-2013; Kutkin, Alexander/M-6085-2013; Lobanov,
Andrei/G-5891-2014; Alakoz, Alexei/M-3667-2015; vinogradov,
igor/M-3773-2015; Kostenko, Vladimir/M-3811-2015; Fedorchuk,
Sergey/M-4285-2015; Shatskaya, Marina/M-4714-2015; Arkhipov,
Mikhail/N-1002-2015; Andreyanov, Vladimir/P-6081-2015; Bychkova,
Vera/M-6114-2015; Pashchenko, Ilya/M-6131-2015; Ponomarev,
Yuri/D-5071-2016; Smirnov, Alexander/D-5073-2016; Belousov,
Konstantin/D-5106-2016; Sakharov, Boris/H-5963-2016; Yakimov,
Vladimir/N-1563-2015; Novikov, Igor/N-5098-2015; Raisanen,
Antti/G-2405-2013; Likhachev, Sergey/M-4705-2015
OI Lisakov, Mikhail/0000-0001-6088-3819; Kovalev, Yuri/0000-0001-9303-3263;
Kutkin, Alexander/0000-0002-1123-7498; Alakoz,
Alexei/0000-0002-8755-5708; Giovannini, Gabriele/0000-0003-4916-6362;
Andreyanov, Vladimir/0000-0001-9695-0104; Bychkova,
Vera/0000-0003-4205-7462;
FU Basic Research Programs of the Presidium of the Russian Academy of
Sciences [P-20, P-21]; Basic Research Programs of the Division of
Physical Sciences of the Russian Academy of Sciences [OFN-16, OFN-17];
Ministry for Education and Science of the Russian Federation
[16.740.11.0155, 8405, 16.518.11.7062, 14.518.11.7054]; Russian
Foundation for Basic Research [10-02-0076, 10-02-00147, 11-02-00368,
12-02-33101]; "Dinastiya" Foundation for Non-Commercial Programs;
national research councils
FX Work on the Early Science Program of the RadioAstron project has been
partially supported by the Basic Research Programs of the Presidium of
the Russian Academy of Sciences P-20 ("The Origin, Structure, and
Evolution of Objects in the Universe") and P-21 ("Non-stationary
Phenomena in Objects of the Universe"), the Basic Research Programs of
the Division of Physical Sciences of the Russian Academy of Sciences
OFN-16 ("Active Processes and Stochastic Structures in the Universe")
and OFN-17 ("Active Processes in Galactic and Extragalactic Objects"),
the Ministry for Education and Science of the Russian Federation, in the
framework of the Federal Targeted Program "Science and Scientific Staff
of Innovative Russia" for 2009-2013 (State contract 16.740.11.0155;
Agreement 8405), the Russian Foundation for Basic Research (projects
10-02-0076, 10-02-00147, 11-02-00368, 12-02-33101), and the "Dinastiya"
Foundation for Non-Commercial Programs. The RATAN-600 observations used
in the analysis of the antenna measurements were supported by the
Ministry for Education and Science of the Russian Federation (State
contracts 16.518.11.7062 and 14.518.11.7054). The European VLBI Network
is a joint facility of European, Chinese, South African and other radio
astronomy institues funded by their national research councils. The
National Radio Astronomy Observatory is a facility of the National
Science Foundation operated under cooperative agrement by Associated
Universities, Inc.
NR 67
TC 38
Z9 41
U1 0
U2 18
PU MAIK NAUKA/INTERPERIODICA/SPRINGER
PI NEW YORK
PA 233 SPRING ST, NEW YORK, NY 10013-1578 USA
SN 1063-7729
J9 ASTRON REP+
JI Astron. Rep.
PD MAR
PY 2013
VL 57
IS 3
BP 153
EP 194
DI 10.1134/S1063772913030025
PG 42
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 129OU
UT WOS:000317851700001
ER
PT J
AU Isaacson, PJ
Petro, NE
Pieters, CM
Besse, S
Boardman, JW
Clark, RN
Green, RO
Lundeen, S
Malaret, E
McLaughlin, S
Sunshine, JM
Taylor, LA
AF Isaacson, Peter J.
Petro, Noah E.
Pieters, Carle M.
Besse, Sebastien
Boardman, Joseph W.
Clark, Roger N.
Green, Robert O.
Lundeen, Sarah
Malaret, Erick
McLaughlin, Stephanie
Sunshine, Jessica M.
Taylor, Lawrence A.
TI Development, importance, and effect of a ground truth correction for the
Moon Mineralogy Mapper reflectance data set
SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS
LA English
DT Article
DE Moon; M3; ground truth; calibration; absorption strength; feldspathic
highlands terrane
ID PROSPECTOR GAMMA-RAY; LUNAR-SURFACE; OPTICAL-PROPERTIES; FINEST
FRACTION; MARE SOILS; SPECTROSCOPY; CLEMENTINE; CRUST; IRON;
CHANDRAYAAN-1
AB We evaluate the effect and importance of a ground truth correction for the Moon Mineralogy Mapper (M-3) level 2 (reflectance) data set. This correction is derived from extensive laboratory characterizations of mature feldspathic lunar soils and is designed to improve the accuracy of 1 mu m absorption features in M-3 reflectance data. To evaluate the correction, the band strength across a subset of the feldspathic highlands terrane (FHT) is analyzed with M-3 imaging spectroscopy data. Using M-3 reflectance data and derived products, we find significant differences in band strength and shape between M-3 observations collected over identical terrain but under different observational and operational conditions. The ground truth correction minimizes these differences in 1 mu m band strengths and also brings the 1 mu m band strengths measured with M-3 data into closer agreement with laboratory measurements of lunar soil samples. Although the FHT region studied was found to have very low band strengths, the M-3 ground truth correction results in overall stronger absorption features for all mature soils relative to uncorrected level 2 (reflectance) data for the same region. These differences between M-3 data collected under different operational conditions and the effects of the ground truth correction, while minor in appearance, can have significant implications for interpretations of any regional soil analyses with M-3 data that rely on absolute 1 mu m absorption feature strength. The M-3 ground truth correction corrects only wavelengths below similar to 1500 nm, and comparisons between corrected and uncorrected wavelengths must be done with caution.
C1 [Isaacson, Peter J.] Univ Hawaii Manoa, Sch Ocean & Earth Sci & Technol, Hawaii Inst Geophys & Planetol, Honolulu, HI 96822 USA.
[Petro, Noah E.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Pieters, Carle M.] Brown Univ, Dept Geol Sci, Providence, RI 02912 USA.
[Besse, Sebastien; McLaughlin, Stephanie; Sunshine, Jessica M.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Boardman, Joseph W.] Analyt Imaging Geophys, Boulder, CO USA.
[Clark, Roger N.] US Geol Survey, Denver, CO 80225 USA.
[Green, Robert O.; Lundeen, Sarah] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Malaret, Erick] Appl Coherent Technol, Herndon, VA USA.
[Taylor, Lawrence A.] Univ Tennessee, Planetary Geosci Inst, Knoxville, TN USA.
RP Isaacson, PJ (reprint author), Univ Hawaii Manoa, Sch Ocean & Earth Sci & Technol, Hawaii Inst Geophys & Planetol, Honolulu, HI 96822 USA.
EM isaacson@higp.hawaii.edu
OI Besse, Sebastien/0000-0002-1052-5439
FU NASA [NNM05AB26C]
FX The efforts of the entire M3 engineering, operations,
science, and data archiving teams are gratefully acknowledged.
M3 science validation is supported through NASA contract
NNM05AB26C. M3 is supported as a NASA Discovery Program
mission of opportunity. The M3 team is grateful to ISRO for
the opportunity to fly as a guest instrument on Chandrayaan-1. The
authors thank Joshua Cahill, Bruce Hapke, and an anonymous reviewer for
their thorough reviews and comments on this manuscript. The manuscript
is much improved thanks to their constructive criticism. This is HIGP
Publication 1919 and SOEST Publication 8539.
NR 70
TC 13
Z9 13
U1 1
U2 10
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-9097
EI 2169-9100
J9 J GEOPHYS RES-PLANET
JI J. Geophys. Res.-Planets
PD MAR
PY 2013
VL 118
IS 3
BP 369
EP 381
DI 10.1002/jgre.20048
PG 13
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 134VJ
UT WOS:000318243300001
ER
PT J
AU Lopes, RMC
Kirk, RL
Mitchell, KL
LeGall, A
Barnes, JW
Hayes, A
Kargel, J
Wye, L
Radebaugh, J
Stofan, ER
Janssen, MA
Neish, CD
Wall, SD
Wood, CA
Lunine, JI
Malaska, MJ
AF Lopes, R. M. C.
Kirk, R. L.
Mitchell, K. L.
LeGall, A.
Barnes, J. W.
Hayes, A.
Kargel, J.
Wye, L.
Radebaugh, J.
Stofan, E. R.
Janssen, M. A.
Neish, C. D.
Wall, S. D.
Wood, C. A.
Lunine, J. I.
Malaska, M. J.
TI Cryovolcanism on Titan: New results from Cassini RADAR and VIMS
SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS
LA English
DT Review
DE Titan; volcanism
ID WATER VOLCANISM; ICY SATELLITES; PLANETOLOGICAL APPLICATIONS; INTERNAL
STRUCTURE; HUYGENS PROBE; LANDING SITE; SOUTH-POLE; SURFACE; AMMONIA;
ENCELADUS
AB The existence of cryovolcanic features on Titan has been the subject of some controversy. Here we use observations from the Cassini RADAR, including Synthetic Aperture Radar (SAR) imaging, radiometry, and topographic data as well as compositional data from the Visible and Infrared Mapping Spectrometer (VIMS) to reexamine several putative cryovolcanic features on Titan in terms of likely processes of origin (fluvial, cryovolcanic, or other). We present evidence to support the cryovolcanic origin of features in the region formerly known as Sotra Facula, which includes the deepest pit so far found on Titan (now known as Sotra Patera), flow-like features (Mohini Fluctus), and some of the highest mountains on Titan (Doom and Erebor Montes). We interpret this region to be a cryovolcanic complex of multiple cones, craters, and flows. However, we find that some other previously supposed cryovolcanic features were likely formed by other processes. Cryovolcanism is still a possible formation mechanism for several features, including the flow-like units in Hotei Regio. We discuss implications for eruption style and composition of cryovolcanism on Titan. Our analysis shows the great value of combining data sets when interpreting Titan's geology and in particular stresses the value of RADAR stereogrammetry when combined with SAR imaging and VIMS.
C1 [Lopes, R. M. C.; Mitchell, K. L.; Janssen, M. A.; Wall, S. D.; Malaska, M. J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Kirk, R. L.] US Geol Survey, Astrogeol Sci Ctr, Flagstaff, AZ 86001 USA.
[LeGall, A.] Univ Versailles St Quentin, Observat Spatiales LATMOS, Atmospheres Lab, Guyancourt, France.
[Barnes, J. W.] Univ Idaho, Dept Phys, Moscow, ID USA.
[Hayes, A.; Lunine, J. I.] Cornell Univ, Dept Astron, Ithaca, NY 14853 USA.
[Kargel, J.] Univ Arizona, Dept Hydrol & Water Resources, Tucson, AZ 85721 USA.
[Wye, L.] Stanford Univ, Dept Geophys, Stanford, CA 94305 USA.
[Wye, L.] Stanford Univ, Dept Elect Engn, Stanford, CA 94305 USA.
[Radebaugh, J.] Brigham Young Univ, Dept Geol Sci, Provo, UT 84602 USA.
[Stofan, E. R.] Proxemy Res, Laytonville, MD USA.
[Neish, C. D.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Wood, C. A.] Planetary Sci Inst, Tucson, AZ USA.
[Wood, C. A.] Wheeling Jesuit Univ, Ctr Educ Technol, Wheeling, WV USA.
RP Lopes, RMC (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM Rosaly.M.Lopes@jpl.nasa.gov
RI Barnes, Jason/B-1284-2009; Neish, Catherine/G-6321-2012; Hayes,
Alexander/P-2024-2014; Lopes, Rosaly/D-1608-2016;
OI Barnes, Jason/0000-0002-7755-3530; Hayes, Alexander/0000-0001-6397-2630;
Lopes, Rosaly/0000-0002-7928-3167; Malaska, Michael/0000-0003-0064-5258
FU National Aeronautics and Space Administration (NASA); NASA
FX Part of this work was carried out at the Jet Propulsion Laboratory,
California Institute of Technology, under contract with the National
Aeronautics and Space Administration (NASA). We thank Sarah Fagents,
Lazlo Kestay, and an anonymous reviewer for comments that greatly
improved the manuscript. We also thank the Cassini-Huygens team for the
design, development, and operation of the mission. The Cassini-Huygens
mission is a joint endeavor of NASA, the European Space Agency (ESA),
and the Italian Space Agency (ASI) and is managed by JPL/Caltech under a
contract with NASA.
NR 109
TC 32
Z9 32
U1 4
U2 39
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-9097
J9 J GEOPHYS RES-PLANET
JI J. Geophys. Res.-Planets
PD MAR
PY 2013
VL 118
IS 3
BP 416
EP 435
DI 10.1002/jgre.20062
PG 20
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 134VJ
UT WOS:000318243300004
ER
PT J
AU Campbell, BA
Putzig, NE
Carter, LM
Morgan, GA
Phillips, RJ
Plaut, JJ
AF Campbell, Bruce A.
Putzig, Nathaniel E.
Carter, Lynn M.
Morgan, Gareth A.
Phillips, Roger. J.
Plaut, Jeffrey J.
TI Roughness and near-surface density of Mars from SHARAD radar echoes
SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS
LA English
DT Article
DE Mars; radar; topography
ID MEDUSAE FOSSAE FORMATION; SCALE ROUGHNESS; MOLA DATA; ICE; SCATTERING;
REFLECTIVITY; TOPOGRAPHY; EVOLUTION; GLACIERS; REGION
AB We present a technique for estimating Mars topographic roughness on horizontal scales from about 10 m to 100 m using Shallow Radar (SHARAD) sounding data. Our results offer a view of surface properties complementary to Mars Orbiter Laser Altimeter (MOLA) pulse-width or baseline roughness maps and can be compared to SHARAD peak-echo properties to infer deviations from the average near-surface density. Latitudinal averaging of SHARAD-derived roughness over Arabia and Noachis Terrae shows good agreement with MOLA-derived roughness and provides clear evidence for latitude-dependent mantling deposits previously inferred from image data. In northwestern Gordii Dorsum, we find that bulk density in at least the upper few meters is significantly lower than in other units of the Medusae Fossae Formation. We observe the same behavior indicative of low near-surface density in wind-eroded crater fill in the southern highlands. Combining surface-properties analysis, subsurface sounding, and high-resolution optical images, we show that the Pavonis Mons fan-shaped deposit differs significantly from lobate debris aprons which SHARAD has shown to be ice-cored. There are no internal radar reflections from the smooth-facies portion of the Pavonis Mons fan-shaped deposit, and we suggest that these deposits are either quite thin or have little dielectric (i.e., density) contrast with the underlying terrain. Future application of these techniques can identify other low-density units across Mars, assist in the mapping of regional volatile-rich mantling units, and provide new constraints on the physical properties of the polar layered terrain.
C1 [Campbell, Bruce A.; Morgan, Gareth A.] Smithsonian Inst, Ctr Earth & Planetary Studies, Washington, DC 20013 USA.
[Putzig, Nathaniel E.; Phillips, Roger. J.] SW Res Inst, Boulder, CO USA.
[Carter, Lynn M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Plaut, Jeffrey J.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
RP Campbell, BA (reprint author), Smithsonian Inst, Ctr Earth & Planetary Studies, MRC 315,POB 37012, Washington, DC 20013 USA.
EM campbellb@si.edu
RI Carter, Lynn/D-2937-2012
FU NASA Mars Reconnaissance Orbiter project
FX The authors thank two anonymous reviewers for their constructive
comments. Funding for this work was provided in part by the NASA Mars
Reconnaissance Orbiter project. The Shallow Radar (SHARAD) was provided
by the Italian Space Agency, and its operations are led by the
Department of Information Engineering, Electronics, and
Telecommunications, University of Rome "La Sapienza."
NR 44
TC 10
Z9 10
U1 1
U2 17
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-9097
EI 2169-9100
J9 J GEOPHYS RES-PLANET
JI J. Geophys. Res.-Planets
PD MAR
PY 2013
VL 118
IS 3
BP 436
EP 450
DI 10.1002/jgre.20050
PG 15
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 134VJ
UT WOS:000318243300005
ER
PT J
AU Hurwitz, DM
Head, JW
Byrne, PK
Xiao, ZY
Solomon, SC
Zuber, MT
Smith, DE
Neumann, GA
AF Hurwitz, Debra M.
Head, James W.
Byrne, Paul K.
Xiao, Zhiyong
Solomon, Sean C.
Zuber, Maria T.
Smith, David E.
Neumann, Gregory A.
TI Investigating the origin of candidate lava channels on Mercury with
MESSENGER data: Theory and observations
SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS
LA English
DT Article
DE thermal erosion; mechanical erosion; sinuous rilles; effusive volcanism
ID SMOOTH PLAINS; WESTERN-AUSTRALIA; MARTIAN CHANNELS; LUNAR; VOLCANISM;
EMPLACEMENT; EROSION; ERUPTION; MARS; VENUS
AB Volcanic plains identified on Mercury are morphologically similar to lunar mare plains but lack constructional and erosional features that are prevalent on other terrestrial planetary bodies. We analyzed images acquired by the MESSENGER spacecraft to identify features on Mercury that may have formed by lava erosion. We used analytical models to estimate eruption flux, erosion rate, and eruption duration to characterize the formation of candidate erosional features, and we compared results with analyses of similar features observed on Earth, the Moon, and Mars. Results suggest that lava erupting at high effusion rates similar to those required to form the Teepee Butte Member of the Columbia River flood basalts (0.1-1.2 x 10(6) m(3) s(-1)) would have been necessary to form wide valleys (>15 km wide) observed in Mercury's northern hemisphere, first by mechanical erosion to remove an upper regolith layer, then by thermal erosion once a lower rigid layer was encountered. Alternatively, results suggest that lava erupting at lower effusion rates similar to those predicted to have formed Rima Prinz on the Moon (4400 m(3) s(-1)) would have been required to form, via thermal erosion, narrower channels (<7 km wide) observed on Mercury. Although these results indicate how erosion might have occurred on Mercury, the observed features may have formed by other processes, including lava flooding terrain sculpted during the formation of the Caloris basin in the case of the wide valleys, or impact melt carving channels into impact ejecta in the case of the narrower channels.
C1 [Hurwitz, Debra M.; Head, James W.] Brown Univ, Dept Geol Sci, Providence, RI 02912 USA.
[Hurwitz, Debra M.] Univ Space Res Assoc, Lunar & Planetary Inst, Houston, TX 77058 USA.
[Byrne, Paul K.; Solomon, Sean C.] Carnegie Inst Sci, Dept Terr Magnetism, Washington, DC USA.
[Xiao, Zhiyong] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA.
[Xiao, Zhiyong] China Univ Geosci Wuhan, Fac Earth Sci, Wuhan, Hunan, Peoples R China.
[Solomon, Sean C.] Columbia Univ, Lamont Doherty Geol Observ, Palisades, NY 10964 USA.
[Zuber, Maria T.; Smith, David E.] MIT, Dept Earth Atmospher & Planetary Sci, Cambridge, MA USA.
[Smith, David E.; Neumann, Gregory A.] NASA, Goddard Space Flight Ctr, Solar Syst Explorat Div, Greenbelt, MD 20771 USA.
RP Hurwitz, DM (reprint author), Univ Space Res Assoc, Lunar & Planetary Inst, Houston, TX 77058 USA.
EM hurwitz@lpi.usra.edu
RI Neumann, Gregory/I-5591-2013
OI Neumann, Gregory/0000-0003-0644-9944
FU NASA Discovery Program [NAS5-97271, NASW-00002]
FX We thank David Hollibaugh Baker and Jay Dickson for their tireless
efforts in downloading and processing MESSENGER data, and we thank Karen
R. Stockstill-Cahill for insightful suggestions during the preparation
of this work. We also thank David A. Williams and Tracy K. P. Gregg for
constructive reviews. Finally, we acknowledge the MESSENGER team for
their ingenuity in getting us to Mercury in the first place. The
MESSENGER project is supported by the NASA Discovery Program under
contracts NAS5-97271 to The Johns Hopkins University Applied Physics
Laboratory and NASW-00002 to the Carnegie Institution of Washington.
NR 84
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U1 0
U2 5
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0148-0227
J9 J GEOPHYS RES-PLANET
JI J. Geophys. Res.-Planets
PD MAR
PY 2013
VL 118
IS 3
BP 471
EP 486
DI 10.1029/2012JE004103
PG 16
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 134VJ
UT WOS:000318243300007
ER
PT J
AU Bishop, JL
Tirsch, D
Tornabene, LL
Jaumann, R
McEwen, AS
McGuire, PC
Ody, A
Poulet, F
Clark, RN
Parente, M
McKeown, NK
Mustard, JF
Murchie, SL
Voigt, J
Aydin, Z
Bamberg, M
Petau, A
Michael, G
Seelos, FP
Hash, CD
Swayze, GA
Neukum, G
AF Bishop, Janice L.
Tirsch, Daniela
Tornabene, Livio L.
Jaumann, Ralf
McEwen, Alfred S.
McGuire, Patrick C.
Ody, Anouck
Poulet, Francois
Clark, Roger N.
Parente, Mario
McKeown, Nancy K.
Mustard, John F.
Murchie, Scott L.
Voigt, Joana
Aydin, Zeynep
Bamberg, Marlene
Petau, Andreas
Michael, Gregory
Seelos, Frank P.
Hash, Christopher D.
Swayze, Gregg A.
Neukum, Gerhard
TI Mineralogy and morphology of geologic units at Libya Montes, Mars:
Ancient aqueously derived outcrops, mafic flows, fluvial features, and
impacts
SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS
LA English
DT Article
DE Mars; remote sensing; mineralogy; reflectance spectroscopy; fluvial
features
ID RESOLUTION REFLECTANCE SPECTROSCOPY; SCIENCE EXPERIMENT HIRISE; EXPRESS
HRSC DATA; INTERIOR CHANNELS; STEREO CAMERA; EVOLUTION; IDENTIFICATION;
CONSTRAINTS; SERPENTINES; DIVERSITY
AB There is ample evidence of both ancient and long-lasting fluvial activity and chemical alteration in the Libya Montes region south of Isidis Basin. The region hosts Noachian to Amazonian aged surface rocks with extensive outcrops of olivine- and pyroxene-bearing material. Libya Montes also features surface outcrops and/or deposits hosting Fe/Mg-smectite, Fe/Mg-smectite mixed with carbonate and/or other Fe/Mg-rich phyllosilicates, and Al-smectite. These units likely formed through chemical alteration connected with hydrothermal activity resulting from the formation of the Isidis Basin and/or the pervasive fluvial activity throughout this region. The morphology and stratigraphy of the aqueous and mafic minerals are described using High Resolution Imaging Science Experiment and High Resolution Stereo Camera derived digital terrain models. Analyses of the Compact Reconnaissance Imaging Spectrometer for Mars spectra show variations in the chemistry of the Fe/Mg-smectite from nontronite-like exposures with spectral features near 2.29 and 2.4 mu m more consistent with Fe23+OH groups in the mineral structure, and saponite-like outcrops with spectral features near 2.31 and 2.38 mu m characteristic of Mg32+OH groups. These Fe/Mg-smectite bearing materials also have bands near 1.9 mu m due to H2O and near 2.5 mu m that could be due to the smectite, other phyllosilicates, and carbonates. All regions exhibiting carbonate features near 3.4-3.5 mu m also have features consistent with the presence of olivine and Fe/Mg-smectite, indicating that the carbonate signatures occur in rocks likely containing a mixture of these minerals. The Al-smectite-bearing rocks have bands near 1.41, 1.91, and 2.19 mu m that are more consistent with beidellite than other Al-phyllosilicates, indicating a higher-temperature or diagenetically processed origin for this material. Our interpretation of the geologic history of this region is that ancient Noachian basaltic crustal materials experienced extensive aqueous alteration at the time of the Isidis impact, during which the montes were also formed, followed by emplacement of a rough olivine-rich lava or melt, and finally the smooth pyroxene-bearing caprock unit.
C1 [Bishop, Janice L.] SETI Inst, Carl Sagan Ctr, Mountain View, CA 94043 USA.
[Bishop, Janice L.] NASA, Ames Res Ctr, Exobiol Branch, Moffett Field, CA 94035 USA.
[Tirsch, Daniela; Jaumann, Ralf; Voigt, Joana; Aydin, Zeynep; Bamberg, Marlene; Petau, Andreas] German Aerosp Ctr DLR, Inst Planetary Res, Berlin, Germany.
[Tornabene, Livio L.] Univ Western Ontario, London, ON, Canada.
[Jaumann, Ralf; Michael, Gregory; Neukum, Gerhard] Free Univ Berlin, Inst Geol Sci, Berlin, Germany.
[McEwen, Alfred S.] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA.
[McGuire, Patrick C.] W Virginia Univ, Dept Chem Engn, Morgantown, WV 26506 USA.
[McGuire, Patrick C.; Murchie, Scott L.; Seelos, Frank P.; Hash, Christopher D.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD USA.
[Ody, Anouck; Poulet, Francois] IAS, Orsay, France.
[Clark, Roger N.; Swayze, Gregg A.] US Geol Survey, Denver, CO 80225 USA.
[Parente, Mario] Univ Massachusetts, Dept Elect & Comp Engn, Amherst, MA 01003 USA.
[McKeown, Nancy K.] Grant MacEwan Univ, Dept Phys Sci, Edmonton, AB, Canada.
[Mustard, John F.] Brown Univ, Dept Geol Sci, Providence, RI 02912 USA.
RP Bishop, JL (reprint author), SETI Inst, Carl Sagan Ctr, Mountain View, CA 94043 USA.
EM jbishop@seti.org
RI Tirsch, Daniela/I-7916-2012; Murchie, Scott/E-8030-2015; McGuire,
Patrick/D-2962-2013; Seelos, Frank/C-7875-2016;
OI Murchie, Scott/0000-0002-1616-8751; McGuire,
Patrick/0000-0001-6592-4966; Seelos, Frank/0000-0001-9721-941X; Tirsch,
Daniela/0000-0001-5905-5426
FU MRO project; NASA-PGG grant; research alliance "Planetary Evolution and
Life"; Lunar Science Institute; NASA's PGG program
FX The authors are grateful to the science and operations teams from MRO
CRISM and HiRISE, Mars Express OMEGA and HRSC for acquiring the data.
Support to several team members from the MRO project and a NASA-PGG
grant are much appreciated. This research has also been partially
supported by the research alliance "Planetary Evolution and Life."
Thanks are also due to E. Cloutis and J. Michalski for helpful reviews
and to NASA's PGG program and Lunar Science Institute for supporting
Brown University's RELAB facility.
NR 79
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U2 14
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-9097
EI 2169-9100
J9 J GEOPHYS RES-PLANET
JI J. Geophys. Res.-Planets
PD MAR
PY 2013
VL 118
IS 3
BP 487
EP 513
DI 10.1029/2012JE004151
PG 27
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 134VJ
UT WOS:000318243300008
ER
PT J
AU Ceamanos, X
Doute, S
Fernando, J
Schmidt, F
Pinet, P
Lyapustin, A
AF Ceamanos, X.
Doute, S.
Fernando, J.
Schmidt, F.
Pinet, P.
Lyapustin, A.
TI Surface reflectance of Mars observed by CRISM/MRO: 1. Multi-angle
Approach for Retrieval of Surface Reflectance from CRISM observations
(MARS-ReCO)
SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS
LA English
DT Article
DE Mars; aerosols; CRISM; MRO; atmospheric correction; surface reflectance;
photometry
ID RADIATIVE-TRANSFER; BIDIRECTIONAL REFLECTANCE; MARTIAN ATMOSPHERE;
OPTICAL DEPTHS; AEROSOL; DUST; ALBEDO; ALGORITHM; LAND; CONSTRAINTS
AB This article addresses the correction for aerosol effects in near-simultaneous multi-angle observations acquired by the Compact Reconnaissance Imaging Spectrometer for Mars (CRISM) aboard the Mars Reconnaissance Orbiter. In the targeted mode, CRISM senses the surface of Mars using 11 viewing angles, which allow it to provide unique information on the scattering properties of surface materials. In order to retrieve these data, however, appropriate strategies must be used to compensate the signal sensed by CRISM for aerosol contribution. This correction is particularly challenging as the photometric curve of these suspended particles is often correlated with the also anisotropic photometric curve of materials at the surface. This article puts forward an innovative radiative transfer-based method named Multi-angle Approach for Retrieval of Surface Reflectance from CRISM Observations (MARS-ReCO). The proposed method retrieves photometric curves of surface materials in reflectance units after removing aerosol contribution. MARS-ReCO represents a substantial improvement regarding previous techniques as it takes into consideration the anisotropy of the surface, thus providing more realistic surface products. Furthermore, MARS-ReCO is fast and provides error bars on the retrieved surface reflectance. The validity and accuracy of MARS-ReCO is explored in a sensitivity analysis based on realistic synthetic data. According to experiments, MARS-ReCO provides accurate results (up to 10% reflectance error) under favorable acquisition conditions. In the companion article, photometric properties of Martian materials are retrieved using MARS-ReCO and validated using in situ measurements acquired during the Mars Exploration Rovers mission.
C1 [Ceamanos, X.; Doute, S.] Univ Grenoble 1, CNRS, IPAG, UMR 5274, Grenoble, France.
[Ceamanos, X.] Meteo France, CNRS, CNRM, GAME, F-31057 Toulouse, France.
[Fernando, J.; Schmidt, F.] Univ Paris 11, Lab IDES, UMR 8148, Orsay, France.
[Fernando, J.; Schmidt, F.] CNRS, F-91405 Orsay, France.
[Pinet, P.] Univ Toulouse, UPS OMP, IRAP, Toulouse, France.
[Pinet, P.] CNRS, IRAP, Toulouse, France.
[Lyapustin, A.] NASA, GSFC, Greenbelt, MD USA.
RP Ceamanos, X (reprint author), Meteo France, CNRS, CNRM, GAME, 42 Ave Gaspard Coriolis, F-31057 Toulouse, France.
EM xavier.ceamanos@meteo.fr
RI Lyapustin, Alexei/H-9924-2014
OI Lyapustin, Alexei/0000-0003-1105-5739
FU "Agence Nationale de la Recherche" (ANR); "Centre National d'Etudes
Spatiales" (CNES); "Centre National de la Recherche Scientifique" (CNRS)
through the "Programme National de Planetologie"
FX This work was done within the framework of the Vahine project funded by
the "Agence Nationale de la Recherche" (ANR) and the "Centre National
d'Etudes Spatiales" (CNES). This work has benefited from the scientific
environment of Paul Sabatier University. We also acknowledge support
from the "Centre National de la Recherche Scientifique" (CNRS) through
the "Programme National de Planetologie". The authors would like to
thank Michael J. Wolff for making his aerosol properties available to
the authors for this study. The authors would like to thank the
anonymous reviewers for their constructive comments that helped
improving this paper.
NR 50
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U1 1
U2 10
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-9097
EI 2169-9100
J9 J GEOPHYS RES-PLANET
JI J. Geophys. Res.-Planets
PD MAR
PY 2013
VL 118
IS 3
BP 514
EP 533
DI 10.1029/2012JE004195
PG 20
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 134VJ
UT WOS:000318243300009
ER
PT J
AU Mischna, MA
Baker, V
Milliken, R
Richardson, M
Lee, C
AF Mischna, Michael A.
Baker, Victor
Milliken, Ralph
Richardson, Mark
Lee, Christopher
TI Effects of obliquity and water vapor/trace gas greenhouses in the early
martian climate
SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS
LA English
DT Article
DE early Mars; sulfur; volcanism; obliquity; greenhouse effect; MarsWRF
ID GENERAL-CIRCULATION MODEL; CARBON-DIOXIDE CLOUDS; EARLY MARS; NORTHERN
PLAINS; ICE; CO2; ATMOSPHERE; VALLEYS; SURFACE; WARM
AB We explore possible mechanisms for the generation of warm, wet climates on early Mars as a result of greenhouse warming by both water vapor and periodic volcanic trace emissions. The presence of both water vapor (a strong greenhouse gas) and other trace greenhouse gases (such as SO2) in a predominantly CO2 atmosphere may act, under certain conditions, to elevate surface temperatures above the freezing point of liquid water, at least episodically. Variations in obliquity are explored to investigate whether these periodic variations in insolation at Mars can broaden the regions or seasons where warm temperatures can exist. We use the Mars Weather Research and Forecasting general circulation model to perform several simulations of the conditions of the early martian atmosphere containing these gases and find global temperatures to be cooler than the elevated levels suggested by at least one recent study by Johnson et al. (2008). While achieving temperatures above 273 K globally remains challenging, the additional warming by greenhouse gases under certain obliquity states can permit for widespread seasonally warm conditions, which can help to explain the presence of fluvial surface features (e.g., valley networks) and hydrous minerals of post-Noachian age, a period when alternate methods do not convincingly explain the sustainability of liquid water. Furthermore, we find that global warming can be achieved with the presence of a darker surface globally, which is consistent with both widespread exposure of unweathered basaltic bedrock or the presence of a large surface ocean or sea.
C1 [Mischna, Michael A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Baker, Victor] Univ Arizona, Dept Planetary Sci, Lunar & Planetary Lab, Tucson, AZ 85721 USA.
[Milliken, Ralph] Brown Univ, Dept Geol Sci, Providence, RI 02912 USA.
[Richardson, Mark; Lee, Christopher] Ashima Res, Pasadena, CA USA.
RP Mischna, MA (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM michael.a.mischna@jpl.nasa.gov
FU NASA High-End Computing Program through the NASA Advanced Supercomputing
Division at Ames Research Center; JPL Office of the Chief Information
Officer; NASA Mars Fundamental Research Program grant [NNH10ZDA001N];
NASA Planetary Atmospheres grant [NNX10AB42G]; National Aeronautics and
Space Administration
FX Resources supporting this work were provided by the NASA High-End
Computing Program through the NASA Advanced Supercomputing Division at
Ames Research Center as well as from the JPL Office of the Chief
Information Officer. MAM, VB, RM, and CL were supported by a NASA Mars
Fundamental Research Program grant NNH10ZDA001N to JPL. Additional
support for CL and MIR was provided by a NASA Planetary Atmospheres
grant NNX10AB42G to Ashima Research. Part of this research was carried
out at the Jet Propulsion Laboratory, California Institute of
Technology, under a contract with the National Aeronautics and Space
Administration.
NR 89
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U1 2
U2 25
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-9097
EI 2169-9100
J9 J GEOPHYS RES-PLANET
JI J. Geophys. Res.-Planets
PD MAR
PY 2013
VL 118
IS 3
BP 560
EP 576
DI 10.1002/jgre.20054
PG 17
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 134VJ
UT WOS:000318243300011
ER
PT J
AU Wilson, LB
Koval, A
Sibeck, DG
Szabo, A
Cattell, CA
Kasper, JC
Maruca, BA
Pulupa, M
Salem, CS
Wilber, M
AF Wilson, L. B., III
Koval, A.
Sibeck, D. G.
Szabo, A.
Cattell, C. A.
Kasper, J. C.
Maruca, B. A.
Pulupa, M.
Salem, C. S.
Wilber, M.
TI Shocklets, SLAMS, and field-aligned ion beams in the terrestrial
foreshock
SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS
LA English
DT Article
ID EARTHS BOW SHOCK; AMPLITUDE MAGNETIC-STRUCTURES; QUASI-PARALLEL SHOCKS;
LOW-FREQUENCY WAVES; UPSTREAM SOLAR-WIND; ISEE-2 OBSERVATIONS;
SUPRATHERMAL IONS; REFLECTED IONS; RE-FORMATION; PLASMA
AB We present Wind spacecraft observations of ion distributions showing field-aligned beams (FABs) and large-amplitude magnetic fluctuations composed of a series of shocklets and short large-amplitude magnetic structures (SLAMS). The FABs are found to have T-b similar to 80 - 850 eV, V-b/V-sw similar to 1.3 - 2.4, T-perpendicular to,T-b/T-parallel to,T-b similar to 1-8, and n(b)/n(o) similar to 0.2-11%. Saturation amplitudes for ion/ion resonant and non-resonant instabilities are too small to explain the observed SLAMS amplitudes. We show two examples where groups of SLAMS can act like a local quasi-perpendicular shock reflecting ions to produce the FABs, a scenario distinct from the more common production at the quasi-perpendicular bow shock. The SLAMS exhibit a foot-like magnetic enhancement with a leading magnetosonic whistler train, consistent with previous observations. Strong ion and electron heating are observed within the series of shocklets and SLAMS with temperatures increasing by factors greater than or similar to 5 and greater than or similar to 3, respectively. Both the core and halo electron components show strong perpendicular heating inside the feature.
C1 [Wilson, L. B., III; Koval, A.; Sibeck, D. G.; Szabo, A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD USA.
[Cattell, C. A.] Univ Minnesota, Sch Phys & Astron, Minneapolis, MN 55455 USA.
[Kasper, J. C.; Maruca, B. A.] Harvard Univ, Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Pulupa, M.; Salem, C. S.; Wilber, M.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
[Koval, A.] Univ Maryland Baltimore Cty, Goddard Planetary Heliophys Inst, Baltimore, MD 21228 USA.
RP Wilson, LB (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD USA.
EM lynn.b.wilsoniii@gmail.com
RI Kasper, Justin/D-1152-2010; Wilson III, Lynn/D-4425-2012;
OI Kasper, Justin/0000-0002-7077-930X; Wilson III,
Lynn/0000-0002-4313-1970; Cattell, Cynthia/0000-0002-3805-320X; Pulupa,
Marc/0000-0002-1573-7457
FU Wind MODA grants; NESSF [NNX07AU72H, NNX07AI05G]; Dr. Leonard
Burlaga/Arctowski Medal Fellowship
FX We thank R. P. Lin (3DP), K. W. Ogilvie (SWE), and R. P. Lepping (MFI)
for the use of data from their instruments. Data from ACE, GOES,
Interball, and OMNI data were obtained from CDAWeb. All data sets from
the Wind spacecraft were produced under Wind MO&DA grants. This research
was supported by NESSF grant NNX07AU72H, grant NNX07AI05G, and the Dr.
Leonard Burlaga/Arctowski Medal Fellowship.
NR 52
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U1 1
U2 6
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-9380
J9 J GEOPHYS RES-SPACE
JI J. Geophys. Res-Space Phys.
PD MAR
PY 2013
VL 118
IS 3
BP 957
EP 966
DI 10.1029/2012JA018186
PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 135FP
UT WOS:000318274000001
ER
PT J
AU DiBraccio, GA
Slavin, JA
Boardsen, SA
Anderson, BJ
Korth, H
Zurbuchen, TH
Raines, JM
Baker, DN
McNutt, RL
Solomon, SC
AF DiBraccio, Gina A.
Slavin, James A.
Boardsen, Scott A.
Anderson, Brian J.
Korth, Haje
Zurbuchen, Thomas H.
Raines, Jim M.
Baker, Daniel N.
McNutt, Ralph L., Jr.
Solomon, Sean C.
TI MESSENGER observations of magnetopause structure and dynamics at Mercury
SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS
LA English
DT Article
ID MINIMUM-VARIANCE ANALYSIS; MAGNETIC-FIELD; BOW SHOCK; DAYSIDE
MAGNETOPAUSE; TERRESTRIAL PLANETS; JOVIAN MAGNETOPAUSE; RECONNECTION
RATE; WIND OBSERVATIONS; 1ST FLYBY; MAGNETOSPHERE
AB On 18 March 2011, MErcury Surface, Space ENvironment, GEochemistry, and Ranging (MESSENGER) became the first spacecraft to orbit Mercury, providing a new opportunity to study the outer boundary of the planet's magnetosphere-the magnetopause. Here we characterize Mercury's magnetopause using measurements collected by MESSENGER's Magnetometer and Fast Imaging Plasma Spectrometer. Analysis of measurements from two of MESSENGER's "hot seasons," when the orbital periapsis is on Mercury's dayside and the magnetopause crossing takes place in the subsolar region, resulted in 43 events with well-determined boundary normals. The typical duration of a magnetopause traversal was similar to 5 s. The average normal magnetic field component was similar to 20 nT, and the dimensionless reconnection rate, i.e., the ratio of the normal magnetic field component to the total field magnitude just inside the magnetopause, was 0.15 +/- 0.02. This rate is a factor of similar to 3 larger than values found during the most extensive surveys at Earth. The ratio of the reconnection rate at Mercury to that of the Earth is comparable to the ratio of the solar wind Alfven speeds at their respective orbits. We also find that the magnetopause reconnection rate at Mercury is independent of magnetic field shear angle, but it varies inversely with plasma beta, the ratio of total thermal pressure to magnetic pressure, in the magnetosheath. These results suggest that reconnection at Mercury is not only more intense than at Earth but also that it occurs for nearly all orientations of the interplanetary magnetic field due to the low-beta nature of the solar wind in the inner heliosphere.
C1 [DiBraccio, Gina A.; Slavin, James A.; Zurbuchen, Thomas H.; Raines, Jim M.] Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA.
[Boardsen, Scott A.] NASA, Goddard Space Flight Ctr, Goddard Planetary Heliophys Inst, Greenbelt, MD 20771 USA.
[Boardsen, Scott A.] Univ Maryland Baltimore Cty, Goddard Planetary Heliophys Inst, Baltimore, MD 21228 USA.
[Anderson, Brian J.; Korth, Haje; McNutt, Ralph L., Jr.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD USA.
[Baker, Daniel N.] Univ Colorado, Atmospher & Space Phys Lab, Boulder, CO 80309 USA.
[Solomon, Sean C.] Carnegie Inst Sci, Dept Terr Magnetism, Washington, DC USA.
[Solomon, Sean C.] Columbia Univ, Lamont Doherty Geol Observ, Palisades, NY 10964 USA.
RP DiBraccio, GA (reprint author), Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA.
EM gdibracc@umich.edu
RI Slavin, James/H-3170-2012; DiBraccio, Gina/C-5960-2014; McNutt,
Ralph/E-8006-2010
OI Slavin, James/0000-0002-9206-724X; McNutt, Ralph/0000-0002-4722-9166
FU NASA [NASW-00002, NAS5-97271]; NASA GSFC Cooperative Education Program
FX The MESSENGER project is supported by the NASA Discovery Program under
contracts NASW-00002 to the Carnegie Institution of Washington and
NAS5-97271 to The Johns Hopkins University Applied Physics Laboratory.
Gina DiBraccio was supported, in part, by the NASA GSFC Cooperative
Education Program.
NR 81
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U1 0
U2 13
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-9380
J9 J GEOPHYS RES-SPACE
JI J. Geophys. Res-Space Phys.
PD MAR
PY 2013
VL 118
IS 3
BP 997
EP 1008
DI 10.1002/jgra.50123
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 135FP
UT WOS:000318274000005
ER
PT J
AU Cramer, WD
Turner, NE
Fok, MC
Buzulukova, NY
AF Cramer, W. D.
Turner, N. E.
Fok, M-C
Buzulukova, N. Y.
TI Effects of different geomagnetic storm drivers on the ring current: CRCM
results
SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS
LA English
DT Article
ID SOLAR-WIND; ENERGETIC PARTICLES; TRAPPED PARTICLES; CURRENT DYNAMICS;
MAGNETIC STORMS; ELECTRIC-FIELDS; PLASMA SHEET; LARGE-SCALE;
MAGNETOSPHERE; DST
AB The storm-time magnetic disturbance at the Earth's equator, as commonly measured by the Dst index, is induced by currents in the near-Earth magnetosphere. The ring current is generally considered the most important contributor, but other magnetospheric currents have also been found to have significant effects. Of the two main types of solar geomagnetic storm drivers, Coronal Mass Ejections (CMEs) tend to have a much greater impact on Dst than Corotating Interaction Regions (CIRs). Ring current models have been found to underestimate Dst, particularly during storms driven by CIRs. One possible explanation is that the models neglect to handle some aspect of ring current physics that is particularly important for CIRs. This study uses the Comprehensive Ring Current Model (CRCM) to estimate the ring current contribution to Dst for a selection of storms of various strengths and different drivers (CMEs and CIRs) that have solar wind parameters that fit a typical profile. The model boundary is set to 10 R-E at the equator, encompassing the entire ring current region. The magnetic field is held fixed, based on average storm parameters, which limits our model results to the effects of convection and plasma sheet density at the model boundary. Our model results generally show good agreement with the size and timing of fluctuations in Dst, which indicates that convection and boundary conditions play an important role in shaping Dst. We also find excellent agreement with the magnitude of Dst for CME-driven storms. For CIR-driven storms, however, the magnitude at the peak of the storm frequently deviates from actual Dst. In general, we agree with the results of previous research that CIR-driven storms are more underpredicted. However, this study includes some weaker CIR-driven storms for which Dst is actually overpredicted. Overall, when examining the dependence of modeled Dst* on actual Dst* at storm peak, we find that there is a statistically significant difference between CME- and CIR-driven storms. We also find that approximately half of the total ring current energy lies beyond an L-value of 6.6. However, this figure could be overestimated due to the use of a static magnetic field, which limits radial transport.
C1 [Cramer, W. D.; Turner, N. E.] Florida Inst Technol, Dept Phys & Space Sci, Melbourne, FL 32901 USA.
[Fok, M-C] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Buzulukova, N. Y.] NASA, Goddard Space Flight Ctr, CRESST, Greenbelt, MD 20771 USA.
[Buzulukova, N. Y.] NASA, Goddard Space Flight Ctr, Geospace Phys Lab, Greenbelt, MD 20771 USA.
[Buzulukova, N. Y.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
RP Cramer, WD (reprint author), Florida Inst Technol, Dept Phys & Space Sci, 150 W Univ Ave, Melbourne, FL 32901 USA.
EM wcramer@my.fit.edu
RI Fok, Mei-Ching/D-1626-2012;
OI Turner, Niescja/0000-0002-3280-4260; Cramer, William/0000-0001-7742-2015
FU NASA [NNX08AT39H]; NSF [0454685, 09-23050]
FX This research was funded though the NASA Graduate Student Researchers
Program Fellowship (Grant No. NNX08AT39H) and the NSF Career Program
(Grant No. 0454685). We thank Hohlmann from the Florida Tech High Energy
Physics group and for use of their computing cluster, Haje Korth for the
use of his IDL Geopack DLM for the Tsyganenko model, and NOAA for their
weekly space weather reports, and we acknowledge the use of the OMNI
solar wind database through CDAWeb. This material is based upon work
supported by the NSF under Grant No. 09-23050. We also thank Ismael Diaz
and Cameo for their helpful comments.
NR 61
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PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-9380
J9 J GEOPHYS RES-SPACE
JI J. Geophys. Res-Space Phys.
PD MAR
PY 2013
VL 118
IS 3
BP 1062
EP 1073
DI 10.1002/jgra.50138
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 135FP
UT WOS:000318274000010
ER
PT J
AU Fung, SF
Hashimoto, K
Kojima, H
Boardsen, SA
Garcia, LN
Matsumoto, H
Green, JL
Reinisch, BW
AF Fung, Shing F.
Hashimoto, Kozo
Kojima, Hirotsugu
Boardsen, Scott A.
Garcia, Leonard N.
Matsumoto, Hiroshi
Green, James L.
Reinisch, Bodo W.
TI Terrestrial myriametric radio burst observed by IMAGE and Geotail
satellites
SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS
LA English
DT Article
ID PLASMA-WAVE OBSERVATIONS; KILOMETRIC CONTINUUM; NONTHERMAL CONTINUUM;
GUIDED ECHOES; RADIATION; MAGNETOSPHERE; EMISSIONS; SPACECRAFT
AB We report the simultaneous detection of a terrestrial myriametric radio burst (TMRB) by IMAGE and Geotail on 19 August 2001. The TMRB was confined in time (0830-1006 UT) and frequency (12-50kHz). Comparisons with all known nonthermal myriametric radiation components reveal that the TMRB might be a distinct radiation with a source that is unrelated to the previously known radiation. Considerations of beaming from spin-modulation analysis and observing satellite and source locations suggest that the TMRB may have a fan beamlike radiation pattern emitted by a discrete, dayside source located along the poleward edge of magnetospheric cusp field lines. TMRB responsiveness to IMF Bz and By orientations suggests that a possible source of the TMRB could be due to dayside magnetic reconnection instigated by northward interplanetary field condition.
C1 [Fung, Shing F.] NASA, Goddard Space Flight Ctr, Geospace Phys Lab, Greenbelt, MD USA.
[Hashimoto, Kozo; Kojima, Hirotsugu] Kyoto Univ, Res Inst Sustainable Humanosphere, Kyoto, Japan.
[Boardsen, Scott A.] NASA, Goddard Space Flight Ctr, Heliophys Sci Div, Greenbelt, MD 20771 USA.
[Boardsen, Scott A.] Univ Maryland, Goddard Planetary Heliophys Inst, Baltimore, MD 21201 USA.
[Garcia, Leonard N.] NASA, Goddard Space Flight Ctr, Wyle, Greenbelt, MD 20771 USA.
[Matsumoto, Hiroshi] Kyoto Univ, Kyoto, Japan.
[Green, James L.] NASA Headquarters, Planetary Sci Div, Washington, DC USA.
[Reinisch, Bodo W.] Lowell Digisonde Int, Lowell, MA USA.
RP Fung, SF (reprint author), NASA, Goddard Space Flight Ctr, Geospace Phys Lab, Greenbelt, MD USA.
EM shing.f.fung@nasa.gov
NR 35
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U1 0
U2 5
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0148-0227
J9 J GEOPHYS RES-SPACE
JI J. Geophys. Res-Space Phys.
PD MAR
PY 2013
VL 118
IS 3
BP 1101
EP 1111
DI 10.1002/jgra.50149
PG 11
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 135FP
UT WOS:000318274000013
ER
PT J
AU Siegel, PH
AF Siegel, Peter H.
TI Untitled
SO IEEE TRANSACTIONS ON TERAHERTZ SCIENCE AND TECHNOLOGY
LA English
DT Editorial Material
C1 [Siegel, Peter H.] CALTECH, Pasadena, CA 91125 USA.
[Siegel, Peter H.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
RP Siegel, PH (reprint author), CALTECH, Pasadena, CA 91125 USA.
NR 0
TC 0
Z9 0
U1 0
U2 2
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 2156-342X
J9 IEEE T THZ SCI TECHN
JI IEEE Trans. Terahertz Sci. Technol.
PD MAR
PY 2013
VL 3
IS 2
BP 125
EP 128
DI 10.1109/TTHZ.2013.2245777
PG 4
WC Engineering, Electrical & Electronic; Optics; Physics, Applied
SC Engineering; Optics; Physics
GA 142BF
UT WOS:000318770300001
ER
PT J
AU Siegel, PH
AF Siegel, Peter H.
TI Terahertz Pioneers A Series of Interviews with Significant Contributors
to Terahertz Science and Technology
SO IEEE TRANSACTIONS ON TERAHERTZ SCIENCE AND TECHNOLOGY
LA English
DT Editorial Material
C1 [Siegel, Peter H.] CALTECH, Dept Biol, Pasadena, CA 91125 USA.
[Siegel, Peter H.] CALTECH, Dept Elect Engn, Pasadena, CA 91125 USA.
[Siegel, Peter H.] NASA, Jet Prop Lab, Pasadena, CA 91125 USA.
RP Siegel, PH (reprint author), CALTECH, Dept Biol, Pasadena, CA 91125 USA.
NR 0
TC 2
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U1 0
U2 2
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 2156-342X
J9 IEEE T THZ SCI TECHN
JI IEEE Trans. Terahertz Sci. Technol.
PD MAR
PY 2013
VL 3
IS 2
BP 129
EP 129
DI 10.1109/TTHZ.2013.2245177
PG 1
WC Engineering, Electrical & Electronic; Optics; Physics, Applied
SC Engineering; Optics; Physics
GA 142BF
UT WOS:000318770300002
ER
PT J
AU Siegel, PH
AF Siegel, Peter H.
TI Terahertz Pioneer: Koji Mizuno "50 Years in Submillimeter-Waves: From
Otaku to Sensei"
SO IEEE TRANSACTIONS ON TERAHERTZ SCIENCE AND TECHNOLOGY
LA English
DT Biographical-Item
C1 [Siegel, Peter H.] CALTECH, Dept Biol, Pasadena, CA 91125 USA.
[Siegel, Peter H.] CALTECH, Dept Elect Engn, Pasadena, CA 91125 USA.
[Siegel, Peter H.] NASA, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Siegel, PH (reprint author), CALTECH, Dept Biol, Pasadena, CA 91125 USA.
EM phs@caltech.edu
NR 1
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U1 0
U2 3
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 2156-342X
J9 IEEE T THZ SCI TECHN
JI IEEE Trans. Terahertz Sci. Technol.
PD MAR
PY 2013
VL 3
IS 2
BP 130
EP 133
DI 10.1109/TTHZ.2013.2245178
PG 4
WC Engineering, Electrical & Electronic; Optics; Physics, Applied
SC Engineering; Optics; Physics
GA 142BF
UT WOS:000318770300003
ER
PT J
AU Tang, A
Chang, MCF
AF Tang, Adrian
Chang, Mau-Chung Frank
TI Inter-Modulated Regenerative CMOS Receivers Operating at 349 and 495 GHz
for THz Imaging Applications
SO IEEE TRANSACTIONS ON TERAHERTZ SCIENCE AND TECHNOLOGY
LA English
DT Article
DE Super-regenerative; THz imaging
AB This paper introduces an ultra-high frequency inter-modulated regenerative receiver (IRR) that operates beyond the maximum oscillation frequency (f(max)) of active devices for terahertz imaging applications. It is accomplished by inter-modulating the fundamental oscillator in a conventional super regenerative receiver (SRR) with a second oscillator to boost the reception frequency. When implemented in 65 nm CMOS technology (f(max)=280GHz), a maximum reception frequency of 349 GHz is achieved. While in 40 nm CMOS technology (f(max)=350GHz), the maximum reception frequency increases to 495 GHz. Multiple received bands are also generated at the alternate inter-modulation frequencies, and enable the possibility of false color THz imaging. The prototype IRR consumes 18.2 mW/pixel and occupies 0.021 mm(2) of silicon area when implemented in 65 nm CMOS technology; and occupies 0.11 mm(2) while consuming 5.6 mW when implemented in 40 nm CMOS technology.
C1 [Tang, Adrian; Chang, Mau-Chung Frank] Univ Calif Los Angeles, Dept Elect Engn, Los Angeles, CA 90025 USA.
RP Tang, A (reprint author), NASA, Jet Prop Lab, Pasadena, CA 91109 USA.
EM Adrian.j.tang@jpl.nasa.gov
NR 11
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U1 2
U2 11
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 2156-342X
J9 IEEE T THZ SCI TECHN
JI IEEE Trans. Terahertz Sci. Technol.
PD MAR
PY 2013
VL 3
IS 2
BP 134
EP 140
DI 10.1109/TTHZ.2012.2225619
PG 7
WC Engineering, Electrical & Electronic; Optics; Physics, Applied
SC Engineering; Optics; Physics
GA 142BF
UT WOS:000318770300004
ER
PT J
AU Lundgren, P
Poland, M
Miklius, A
Orr, T
Yun, SH
Fielding, E
Liu, Z
Tanaka, A
Szeliga, W
Hensley, S
Owen, S
AF Lundgren, Paul
Poland, Michael
Miklius, Asta
Orr, Tim
Yun, Sang-Ho
Fielding, Eric
Liu, Zhen
Tanaka, Akiko
Szeliga, Walter
Hensley, Scott
Owen, Susan
TI Evolution of dike opening during the March 2011 Kamoamoa fissure
eruption, Kilauea Volcano, Hawai'i
SO JOURNAL OF GEOPHYSICAL RESEARCH-SOLID EARTH
LA English
DT Article
ID RIFT ZONES; RADAR INTERFEROMETRY; SURFACE DEFORMATION; SATELLITE RADAR;
SOUTH FLANK; HECTOR MINE; INTRUSION; MODEL; GPS; EARTHQUAKE
AB The 5-9 March 2011 Kamoamoa fissure eruption along the east rift zone of Kilauea Volcano, Hawai'i, followed months of pronounced inflation at Kilauea summit. We examine dike opening during and after the eruption using a comprehensive interferometric synthetic aperture radar (InSAR) data set in combination with continuous GPS data. We solve for distributed dike displacements using a whole Kilauea model with dilating rift zones and possibly a deep decollement. Modeled surface dike opening increased from nearly 1.5 m to over 2.8 m from the first day to the end of the eruption, in agreement with field observations of surface fracturing. Surface dike opening ceased following the eruption, but subsurface opening in the dike continued into May 2011. Dike volumes increased from 15, to 16, to 21 million cubic meters (MCM) after the first day, eruption end, and 2 months following, respectively. Dike shape is distinctive, with a main limb plunging from the surface to 2-3 km depth in the up-rift direction toward Kilauea's summit, and a lesser projection extending in the down-rift direction toward Pu'u 'O'o at 2 km depth. Volume losses beneath Kilauea summit (1.7 MCM) and Pu'u 'O'o (5.6 MCM) crater, relative to dike plus erupted volume (18.3 MCM), yield a dike to source volume ratio of 2.5 that is in the range expected for compressible magma without requiring additional sources. Inflation of Kilauea's summit in the months before the March 2011 eruption suggests that the Kamoamoa eruption resulted from overpressure of the volcano's magmatic system.
C1 [Lundgren, Paul; Yun, Sang-Ho; Fielding, Eric; Liu, Zhen; Hensley, Scott; Owen, Susan] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Poland, Michael; Miklius, Asta; Orr, Tim] US Geol Survey, Hawaiian Volcano Observ, Hawaiian Volcanoes Natl, HI USA.
[Tanaka, Akiko] AIST, Geol Survey Japan, Tsukuba, Ibaraki, Japan.
[Szeliga, Walter] Cent Washington Univ, Dept Geol Sci, Ellensburg, WA USA.
RP Lundgren, P (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr,MS 300-233, Pasadena, CA 91109 USA.
EM Paul.R.Lundgren@jpl.nasa.gov
RI Fielding, Eric/A-1288-2007; Liu, Zhen/D-8334-2017;
OI Fielding, Eric/0000-0002-6648-8067; Poland, Michael/0000-0001-5240-6123
FU Italian Space Agency (ASI) [ID 2270]; Hawaii Supersite project
[GEO0875]; National Aeronautics and Space Administration at the Jet
Propulsion Laboratory, California Institute of Technology
FX The COSMO-SkyMed data were provided courtesy of the Italian Space Agency
(ASI) under CSK AO Project ID 2270. The German Aerospace Center (DLR)
TerraSAR-X data were courtesy of the Hawaii Supersite project GEO0875.
ALOS PALSAR data were provided courtesy of the Japan Aerospace
Exploration Agency (JAXA), Minestry of Economy, Trade and Industry
(METI), which were distributed by the Earth Remote Sensing Data Analysis
Center (ERSDAC). METI and JAXA retain ownership of the original ALOS
PALSAR data. UAVSAR data were provided by the UAVSAR Project, JPL, with
special thanks to Y. Zheng, Y. Lou, the radar operations personnel at
JPL, and T. Moes and the flight operations personnel at NASA Dryden
Flight Research Center. Maps in Figure 1 were generated using the public
domain Generic Mapping Tools (GMT) software [Wessel and Smith, 1995].
Critical reviews from two anonymous reviewers and C. Wicks greatly
improved the manuscript. Original TerraSAR-X data is copyright (2011)
DLR. Original COSMO-SkyMed data copyright (2010, 2011). The research
described in this paper was supported under contract with the National
Aeronautics and Space Administration at the Jet Propulsion Laboratory,
California Institute of Technology.
NR 49
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PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0148-0227
J9 J GEOPHYS RES-SOL EA
JI J. Geophys. Res.-Solid Earth
PD MAR
PY 2013
VL 118
IS 3
BP 897
EP 914
DI 10.1002/jgrb.50108
PG 18
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 135FK
UT WOS:000318273300008
ER
PT J
AU Han, SC
Riva, R
Sauber, J
Okal, E
AF Han, Shin-Chan
Riva, Riccardo
Sauber, Jeanne
Okal, Emile
TI Source parameter inversion for recent great earthquakes from a
decade-long observation of global gravity fields
SO JOURNAL OF GEOPHYSICAL RESEARCH-SOLID EARTH
LA English
DT Article
ID SUMATRA-ANDAMAN EARTHQUAKE; LOCALIZED SPECTRAL-ANALYSIS; LAYERED
SPHERICAL EARTH; SURFACE MASS LOADS; DETERMINING DEFORMATION; CRUSTAL
DEFORMATION; TOHOKU EARTHQUAKE; FREE OSCILLATIONS; GREENS FUNCTION;
NORMAL-MODES
AB We quantify gravity changes after great earthquakes present within the 10 year long time series of monthly Gravity Recovery and Climate Experiment (GRACE) gravity fields. Using spherical harmonic normal-mode formulation, the respective source parameters of moment tensor and double-couple were estimated. For the 2004 Sumatra-Andaman earthquake, the gravity data indicate a composite moment of 1.2 x 10(23) N m with a dip of 10 degrees, in agreement with the estimate obtained at ultralong seismic periods. For the 2010 Maule earthquake, the GRACE solutions range from 2.0 to 2.7 x 10(22) N m for dips of 12 degrees-24 degrees and centroid depths within the lower crust. For the 2011 Tohoku-Oki earthquake, the estimated scalar moments range from 4.1 to 6.1 x 10(22) N m, with dips of 9 degrees-19 degrees and centroid depths within the lower crust. For the 2012 Indian Ocean strike-slip earthquakes, the gravity data delineate a composite moment of 1.9 x 10(22) N m regardless of the centroid depth, comparing favorably with the total moment of the main ruptures and aftershocks. The smallest event we successfully analyzed with GRACE was the 2007 Bengkulu earthquake with M-0 similar to 5.0 x 10(21) N m. We found that the gravity data constrain the focal mechanism with the centroid only within the upper and lower crustal layers for thrust events. Deeper sources (i.e., in the upper mantle) could not reproduce the gravity observation as the larger rigidity and bulk modulus at mantle depths inhibit the interior from changing its volume, thus reducing the negative gravity component. Focal mechanisms and seismic moments obtained in this study represent the behavior of the sources on temporal and spatial scales exceeding the seismic and geodetic spectrum. Citation: Han, S.-C., R. Riva, J. Sauber, and E. Okal (2013), Source parameter inversion for recent great earthquakes from a decade-long observation of global gravity fields, J. Geophys. Res. Solid Earth, 118, 1240-1267, doi: 10.1002/jgrb.50116.
C1 [Han, Shin-Chan; Sauber, Jeanne] NASA, Goddard Space Flight Ctr, Planetary Geodynam Lab, Greenbelt, MD USA.
[Riva, Riccardo] Delft Univ Technol, Dept Geosci & Remote Sensing, Delft, Netherlands.
[Okal, Emile] Northwestern Univ, Dept Earth & Planetary Sci, Evanston, IL USA.
RP Han, SC (reprint author), NASA, Goddard Space Flight Ctr, Planetary Geodynam Lab, Greenbelt, MD USA.
EM shin-chan.han@nasa.gov
RI Han, Shin-Chan/A-2022-2009
FU NASA Earth Surface and Interior program; GRACE project
FX This work was supported by the NASA Earth Surface and Interior program
and the GRACE project. We thank DLR for providing the GRACE telemetry
data and JPL and CSR for producing the high-quality level 1B and level 2
products. We thank Fred Pollitz, Richard Gross, Erik Ivins, Caroline de
Linage, Luis Rivera, and Frederik Simons for helpful discussions. We
thank two anonymous reviewers and an associate editor for the
constructive comments to improve our original manuscript.
NR 78
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PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-9313
EI 2169-9356
J9 J GEOPHYS RES-SOL EA
JI J. Geophys. Res.-Solid Earth
PD MAR
PY 2013
VL 118
IS 3
BP 1240
EP 1267
DI 10.1002/jgrb.50116
PG 28
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 135FK
UT WOS:000318273300034
ER
PT J
AU Keith, MJ
Coles, W
Shannon, RM
Hobbs, GB
Manchester, RN
Bailes, M
Bhat, NDR
Burke-Spolaor, S
Champion, DJ
Chaudhary, A
Hotan, AW
Khoo, J
Kocz, J
Oslowski, S
Ravi, V
Reynolds, JE
Sarkissian, J
van Straten, W
Yardley, DRB
AF Keith, M. J.
Coles, W.
Shannon, R. M.
Hobbs, G. B.
Manchester, R. N.
Bailes, M.
Bhat, N. D. R.
Burke-Spolaor, S.
Champion, D. J.
Chaudhary, A.
Hotan, A. W.
Khoo, J.
Kocz, J.
Oslowski, S.
Ravi, V.
Reynolds, J. E.
Sarkissian, J.
van Straten, W.
Yardley, D. R. B.
TI Measurement and correction of variations in interstellar dispersion in
high-precision pulsar timing
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE methods: data analysis; pulsars: general; ISM: structure
ID MILLISECOND PULSARS; MAGNETIC-FIELD; SCATTERING; LIMITS; ARRAY;
SCINTILLATION; PACKAGE; TEMPO2; WAVES
AB Signals from radio pulsars show a wavelength-dependent delay due to dispersion in the interstellar plasma. At a typical observing wavelength, this delay can vary by tens of microseconds on 5-yr time-scales, far in excess of signals of interest to pulsar timing arrays, such as that induced by a gravitational wave background. Measurement of these delay variations is not only crucial for the detection of such signals, but also provides an unparalleled measurement of the turbulent interstellar plasma at astronomical unit (au) scales.
In this paper we demonstrate that without consideration of wavelength-independent red noise, 'simple' algorithms to correct for interstellar dispersion can attenuate signals of interest to pulsar timing arrays. We present a robust method for this correction, which we validate through simulations, and apply it to observations from the Parkes Pulsar Timing Array. Correction for dispersion variations comes at a cost of increased band-limited white noise. We discuss scheduling to minimize this additional noise, and factors, such as scintillation, that can exacerbate the problem.
Comparison with scintillation measurements confirms previous results that the spectral exponent of electron density variations in the interstellar medium often appears steeper than expected. We also find a discrete change in dispersion measure of PSR J1603-7202 of similar to 2 x 10(-3) cm(-3) pc for about 250 d. We speculate that this has a similar origin to the 'extreme scattering events' seen in other sources. In addition, we find that four pulsars show a wavelength-dependent annual variation, indicating a persistent gradient of electron density on an au spatial scale, which has not been reported previously.
C1 [Keith, M. J.; Shannon, R. M.; Hobbs, G. B.; Manchester, R. N.; Chaudhary, A.; Hotan, A. W.; Khoo, J.; Oslowski, S.; Ravi, V.; Reynolds, J. E.; Sarkissian, J.; Yardley, D. R. B.] CSIRO Astron & Space Sci, Australia Telescope Natl Facil, Epping, NSW 1710, Australia.
[Coles, W.] Univ Calif San Diego, La Jolla, CA 92093 USA.
[Bailes, M.; Bhat, N. D. R.; Kocz, J.; Oslowski, S.; van Straten, W.] Swinburne Univ Technol, Ctr Astrophys & Supercomp, Hawthorn, Vic 3122, Australia.
[Bhat, N. D. R.] Curtin Univ Technol, Int Ctr Radio Astron Res, Bentley, WA 6102, Australia.
[Burke-Spolaor, S.] CALTECH, Jet Prop Lab, NASA, Pasadena, CA 91109 USA.
[Champion, D. J.] Max Planck Inst Radioastron, D-53121 Bonn, Germany.
[Kocz, J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Ravi, V.] Univ Melbourne, Sch Phys, Melbourne, Vic 3010, Australia.
[Yardley, D. R. B.] Univ Sydney, Sch Phys A29, Sydney Inst Astron, Sydney, NSW 2006, Australia.
RP Keith, MJ (reprint author), CSIRO Astron & Space Sci, Australia Telescope Natl Facil, POB 76, Epping, NSW 1710, Australia.
EM mkeith@pulsarastronomy.net
OI Champion, David/0000-0003-1361-7723; Shannon, Ryan/0000-0002-7285-6348;
Kocz, Jonathon/0000-0003-0249-7586; van Straten,
Willem/0000-0003-2519-7375; Oslowski, Stefan/0000-0003-0289-0732
FU Australian Research Council [DP0878388, FF0348478]; Commonwealth of
Australia
FX This work has been carried out as part of the Parkes Pulsar Timing Array
project. GBH is the recipient of an Australian Research Council QEII
Fellowship (project DP0878388), the PPTA project was initiated with
support from RNM's Federation Fellowship (FF0348478). The Parkes radio
telescope is part of the Australia Telescope which is funded by the
Commonwealth of Australia for operation as a National Facility managed
by CSIRO.
NR 32
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U1 0
U2 1
PU OXFORD UNIV PRESS
PI OXFORD
PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND
SN 0035-8711
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD MAR
PY 2013
VL 429
IS 3
BP 2161
EP 2174
DI 10.1093/mnras/sts486
PG 14
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 135ET
UT WOS:000318271300021
ER
PT J
AU Littenberg, TB
Larson, SL
Nelemans, G
Cornish, NJ
AF Littenberg, T. B.
Larson, S. L.
Nelemans, G.
Cornish, N. J.
TI Prospects for observing ultracompact binaries with space-based
gravitational wave interferometers and optical telescopes
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE gravitational waves; binaries: close; white dwarfs; Galaxy: stellar
content
ID WHITE-DWARF BINARIES; RADIATION; GALAXIES; SYSTEMS; SIGNAL
AB Space-based gravitational wave interferometers are sensitive to the galactic population of ultracompact binaries. An important subset of the ultracompact binary population are those stars that can be individually resolved by both gravitational wave interferometers and electromagnetic telescopes. The aim of this paper is to quantify the multimessenger potential of space-based interferometers with arm-lengths between 1 and 5 Gm. The Fisher information matrix is used to estimate the number of binaries from a model of the Milky Way which are localized on the sky by the gravitational wave detector to within 1 and 10 deg(2) and bright enough to be detected by a magnitude-limited survey. We find, depending on the choice of GW detector characteristics, limiting magnitude and observing strategy, that up to several hundred gravitational wave sources could be detected in electromagnetic follow-up observations.
C1 [Littenberg, T. B.] Univ Maryland, Dept Phys, Maryland Ctr Fundamental Phys, College Pk, MD 20742 USA.
[Littenberg, T. B.] NASA, Goddard Space Flight Ctr, Gravitat Astrophys Lab, Greenbelt, MD 20771 USA.
[Larson, S. L.] Utah State Univ, Dept Phys, Logan, UT 84322 USA.
[Nelemans, G.] Radboud Univ Nijmegen, Dept Astrophys, NL-6500 GL Nijmegen, Netherlands.
[Nelemans, G.] Katholieke Univ Leuven, Inst Astron, B-3001 Louvain, Belgium.
[Nelemans, G.] Nikhef, NL-1098 XG Amsterdam, Netherlands.
[Cornish, N. J.] Montana State Univ, Dept Phys, Bozeman, MT 59717 USA.
RP Littenberg, TB (reprint author), Univ Maryland, Dept Phys, Maryland Ctr Fundamental Phys, College Pk, MD 20742 USA.
EM tyson.b.littenberg@nasa.gov
RI Nelemans, Gijs/D-3177-2012
OI Nelemans, Gijs/0000-0002-0752-2974
FU NASA [08-ATFP08-0126, NNX12AG30G, NNX10AH15G]; Dutch Foundation for
Fundamental Research on Matter (FOM)
FX This work was supported by NASA Grants 08-ATFP08-0126 (TBL), NNX12AG30G
(SLL) and NNX10AH15G (NJC). GN acknowledges support from the Dutch
Foundation for Fundamental Research on Matter (FOM).
NR 38
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U1 0
U2 1
PU OXFORD UNIV PRESS
PI OXFORD
PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND
SN 0035-8711
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD MAR
PY 2013
VL 429
IS 3
BP 2361
EP 2365
DI 10.1093/mnras/sts507
PG 5
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 135ET
UT WOS:000318271300036
ER
PT J
AU Fuller, J
Derekas, A
Borkovits, T
Huber, D
Bedding, TR
Kiss, LL
AF Fuller, Jim
Derekas, A.
Borkovits, T.
Huber, D.
Bedding, T. R.
Kiss, L. L.
TI Tidally induced oscillations and orbital decay in compact triple-star
systems
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE binaries: close; binaries: eclipsing; stars: individual: HD 181068;
stars: oscillations
ID SOLAR-LIKE OSCILLATIONS; PSR J0045-7319 BINARY; RED GIANT STARS; 1ST 4
MONTHS; HIERARCHICAL TRIPLE; KEPLER DATA; DYNAMICAL TIDES; EVOLUTION;
ASTEROSEISMOLOGY; KOI-54
AB We investigate the nature of tidal effects in compact triple-star systems. The hierarchical structure of a triple system produces tidal forcing at high frequencies unobtainable in binary systems, allowing for the tidal excitation of high-frequency p-modes in the stellar components. The tidal forcing exists even for circular, aligned and synchronized systems. We calculate the magnitude and frequencies of three-body tidal forcing on the central primary star for circular and coplanar orbits, and we estimate the amplitude of the tidally excited oscillation modes. We also calculate the secular orbital changes induced by the tidally excited modes and show that they can cause significant orbital decay. During certain phases of stellar evolution, the tidal dissipation may be greatly enhanced by resonance locking. We then compare our theory to observations of HD 181068, which is a hierarchical triply eclipsing star system in the Kepler field of view. The observed oscillation frequencies in HD 181068 can be naturally explained by three-body tidal effects. We then compare the observed oscillation amplitudes and phases in HD 181068 to our predictions, finding mostly good agreement. Finally, we discuss the past and future evolution of compact triple systems like HD 181068.
C1 [Fuller, Jim] Cornell Univ, Ctr Space Res, Dept Astron, Ithaca, NY 14853 USA.
[Derekas, A.; Borkovits, T.; Kiss, L. L.] Hungarian Acad Sci, Res Ctr Astron & Earth Sci, Konkoly Observ, H-1121 Budapest, Hungary.
[Derekas, A.; Huber, D.; Bedding, T. R.; Kiss, L. L.] Univ Sydney, Sch Phys, Sydney Inst Astron, Sydney, NSW 2006, Australia.
[Borkovits, T.] Baja Astron Observ, H-6500 Baja, Hungary.
[Borkovits, T.; Kiss, L. L.] ELTE Gothard Lendulet Res Grp, H-9700 Szombathely, Hungary.
[Huber, D.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
RP Fuller, J (reprint author), Cornell Univ, Ctr Space Res, Dept Astron, Ithaca, NY 14853 USA.
EM jwf75@cornell.edu
RI Derekas, Aliz/G-2091-2016;
OI Derekas, Aliz/0000-0002-6526-9444; Bedding, Timothy/0000-0001-5943-1460;
Bedding, Tim/0000-0001-5222-4661
FU NSF [11-Astro11F-0016, AST-1008245, AST-1211061]; NASA [NNX12AF85G,
NNX10AP19G]; Hungarian OTKA Grants [K76816, K83790, MB08C 81013];
Hungarian Academy of Sciences; European Research Council under the
European Community [227224]; Magyary Zoltan Public Foundation; Hungarian
Eotvos fellowship; European Community [269194]
FX We thank Dong Lai and Dan Tamayo for useful discussions. JF acknowledges
the hospitality (autumn 2011) of the Kavli Institute for Theoretical
Physics at UCSB (funded by the NSF through Grant 11-Astro11F-0016) where
part of the work was carried out. This project has been supported by NSF
grants AST-1008245 and AST-1211061, NASA grants NNX12AF85G and
NNX10AP19G, the Hungarian OTKA Grants K76816, K83790 and MB08C 81013 and
the 'Lendulet-2009' Young Researchers Programme of the Hungarian Academy
of Sciences. Part of the research leading to these results has received
funding from the European Research Council under the European
Community's Seventh Framework Programme (FP7/2007-2013)/ERC grant
agreement no. 227224 (PROSPERITY). AD gratefully acknowledges financial
support from the Magyary Zoltan Public Foundation. AD was supported by
the Hungarian Eotvos fellowship. AD has been supported by the Janos
Bolyai Research Scholarship of the Hungarian Academy of Sciences. LLK
wishes to thank support from the European Community's Seventh Framework
Programme (FP7/2007-2013) under grant agreement no. 269194. The Kepler
Team and the Kepler Guest Observer Office are recognized for helping to
make the mission and these data possible.
NR 44
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PI OXFORD
PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND
SN 0035-8711
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD MAR
PY 2013
VL 429
IS 3
BP 2425
EP 2441
DI 10.1093/mnras/sts511
PG 17
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 135ET
UT WOS:000318271300042
ER
PT J
AU Sidoli, L
Esposito, P
Sguera, V
Bodaghee, A
Tomsick, JA
Pottschmidt, K
Rodriguez, J
Romano, P
Wilms, J
AF Sidoli, L.
Esposito, P.
Sguera, V.
Bodaghee, A.
Tomsick, J. A.
Pottschmidt, K.
Rodriguez, J.
Romano, P.
Wilms, J.
TI A Suzaku X-ray observation of one orbit of the supergiant fast X-ray
transient IGR J16479-4514
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE accretion, accretion discs; X-rays: binaries; supergiants; X-rays:
individual: IGR J16479-4514
ID XMM-NEWTON; MULTIWAVELENGTH OBSERVATIONS; INTEGRAL OBSERVATIONS;
INTERSTELLAR-MEDIUM; SPECTRAL-ANALYSIS; COMPANION STAR; STELLAR WINDS;
BINARIES; ACCRETION; OUTBURST
AB We report on a 250 ks long X-ray observation of the supergiant fast X-ray transient IGR J16479-4514 performed with Suzaku in 2012 February. During this observation, about 80 per cent of the short orbital period (P-orb similar to 3.32 d) was covered as continuously as possible for the first time. The source light curve displays variability of more than two orders of magnitude, starting with a very low emission state (10(-13) erg cm(-2) s(-1); 1-10 keV) lasting the first 46 ks, consistent with being due to the X-ray eclipse by the supergiant companion. The transition to the uneclipsed X-ray emission is energy dependent. Outside the eclipse, the source spends most of the time at a level of 6-7 x 10(-12) erg cm(-2) s(-1) punctuated by two structured faint flares with a duration of about 10 and 15 ks, respectively, reaching a peak flux of 3-4 x 10(-11) erg cm(-2) s(-1), separated by about 0.2 in orbital phase. Remarkably, the first faint flare occurs at a similar orbital phase of the bright flares previously observed in the system. This indicates the presence of a phase-locked large-scale structure in the supergiant wind, driving a higher accretion rate on to the compact object. The average X-ray spectrum is hard and highly absorbed, with a column density, N-H, of 1023 cm-2, clearly in excess of the interstellar absorption. There is no evidence for variability of the absorbing column density, except that during the eclipse, where a less absorbed X-ray spectrum is observed. A narrow Fe K alpha emission line at 6.4 keV is viewed along the whole orbit, with an intensity which correlates with the continuum emission above 7 keV. The scattered component visible during the X-ray eclipse allowed us to directly probe the wind density at the orbital separation, resulting in rho(w) = 7 x 10(-14) g cm(-3). Assuming a spherical geometry for the supergiant wind, the derived wind density translates into a ratio. M-w/v(infinity) = 7 x 10(-17) M-circle dot km(-1) which, assuming terminal velocities in a large range 500-3000 km s(-1), implies an accretion luminosity two orders of magnitude higher than that observed. As a consequence, a mechanism should be at work reducing the mass accretion rate. Different possibilities are discussed.
C1 [Sidoli, L.; Esposito, P.] Ist Astrofis Spaziale & Fis Cosm, INAF, I-20133 Milan, Italy.
[Sguera, V.] Ist Astrofis Spaziale & Fis Cosm, INAF, I-40129 Bologna, Italy.
[Bodaghee, A.; Tomsick, J. A.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
[Pottschmidt, K.] CRESST, Greenbelt, MD 20771 USA.
[Pottschmidt, K.] NASA Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA.
[Pottschmidt, K.] Univ Maryland Baltimore Cty, Ctr Space Sci & Technol, Baltimore, MD 21250 USA.
[Rodriguez, J.] CEA IRFU Univ Paris Diderot CNRS INSU, CEA DSM IRFU SAp, Lab AIM, Ctr Saclay, F-91191 Gif Sur Yvette, France.
[Romano, P.] Ist Astrofis Spaziale & Fis Cosm, INAF, I-90146 Palermo, Italy.
[Wilms, J.] Univ Erlangen Nurnberg, Dr Karl Remeis Sternwarte & Erlangen Ctr Astropar, D-96049 Bamberg, Germany.
RP Sidoli, L (reprint author), Ist Astrofis Spaziale & Fis Cosm, INAF, Via E Bassini 15, I-20133 Milan, Italy.
EM sidoli@iasf-milano.inaf.it
RI XRAY, SUZAKU/A-1808-2009;
OI Sidoli, Lara/0000-0001-9705-2883; Rodriguez, Jerome/0000-0002-4151-4468;
Esposito, Paolo/0000-0003-4849-5092; Wilms, Joern/0000-0003-2065-5410;
sguera, vito/0000-0001-8202-9381
FU PRIN-INAF; NASA [11-ADAP11-0227]
FX This work is based on data from observations with Suzaku. This work was
supported by the grant from PRIN-INAF 2009, 'The transient X-ray sky:
new classes of X-ray binaries containing neutron stars' (PI: L. Sidoli).
AB received funding from NASA grant 11-ADAP11-0227. LS is grateful to
Angela Bazzano and Tim Oosterbroek for very helpful comments and
suggestions. PE thanks Sara Motta for fruitful discussions. This
research has made use of the IGR Sources page maintained by J. Rodriguez
and A. Bodaghee (http://irfu.cea.fr/Sap/IGR-Sources/).
NR 48
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PI OXFORD
PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND
SN 0035-8711
EI 1365-2966
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD MAR
PY 2013
VL 429
IS 3
BP 2763
EP 2771
DI 10.1093/mnras/sts559
PG 9
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 135ET
UT WOS:000318271300071
ER
PT J
AU Burr, DM
Perron, JT
Lamb, MP
Irwin, RP
Collins, GC
Howard, AD
Sklar, LS
Moore, JM
Adamkovics, M
Baker, VR
Drummond, SA
Black, BA
AF Burr, Devon M.
Perron, J. Taylor
Lamb, Michael P.
Irwin, Rossman P., III
Collins, Geoffrey C.
Howard, Alan D.
Sklar, Leonard S.
Moore, Jeffrey M.
Adamkovics, Mate
Baker, Victor R.
Drummond, Sarah A.
Black, Benjamin A.
TI Fluvial features on Titan: Insights from morphology and modeling
SO GEOLOGICAL SOCIETY OF AMERICA BULLETIN
LA English
DT Article
ID HUYGENS LANDING SITE; UNIDIRECTIONAL WATER FLOWS; CASSINI RADAR; RIVER
INCISION; SEDIMENT TRANSPORT; SOUTH-POLE; BED CONFIGURATIONS; TERMINAL
VELOCITY; TECTONIC ACTIVITY; METHANE CYCLE
AB Fluvial features on Titan have been identified in synthetic aperture radar (SAR) data taken during spacecraft flybys by the Cassini Titan Radar Mapper (RADAR) and in Descent Imager/Spectral Radiometer (DISR) images taken during descent of the Huygens probe to the surface. Interpretations using terrestrial analogs and process mechanics extend our perspective on fluvial geomorphology to another world and offer insight into their formative processes. At the landscape scale, the varied morphologies of Titan's fluvial networks imply a variety of mechanical controls, including structural influence, on channelized flows. At the reach scale, the various morphologies of individual fluvial features, implying a broad range of fluvial processes, suggest that (paleo-)flows did not occupy the entire observed width of the features. DISR images provide a spatially limited view of uplands dissected by valley networks, also likely formed by overland flows, which are not visible in lower-resolution SAR data. This high-resolution snapshot suggests that some fluvial features observed in SAR data may be river valleys rather than channels, and that uplands elsewhere on Titan may also have fine-scale fluvial dissection that is not resolved in SAR data. Radar-bright terrain with crenulated bright and dark bands is hypothesized here to be a signature of fine-scale fluvial dissection. Fluvial deposition is inferred to occur in braided channels, in (paleo)lake basins, and on SAR-dark plains, and DISR images at the surface indicate the presence of fluvial sediment. Flow sufficient to move sediment is inferred from observations and modeling of atmospheric processes, which support the inference from surface morphology of precipitation-fed fluvial processes. With material properties appropriate for Titan, terrestrial hydraulic equations are applicable to flow on Titan for fully turbulent flow and rough boundaries. For low-Reynolds-number flow over smooth boundaries, however, knowledge of fluid kinematic viscosity is necessary. Sediment movement and bed form development should occur at lower bed shear stress on Titan than on Earth. Scaling bedrock erosion, however, is hampered by uncertainties regarding Titan material properties. Overall, observations of Titan point to a world pervasively influenced by fluvial processes, for which appropriate terrestrial analogs and formulations may provide insight.
C1 [Burr, Devon M.; Drummond, Sarah A.] Univ Tennessee, Dept Earth & Planetary Sci, Knoxville, TN 37996 USA.
[Perron, J. Taylor; Black, Benjamin A.] MIT, Dept Earth Atmospher & Planetary Sci, Cambridge, MA 02139 USA.
[Lamb, Michael P.] CALTECH, Pasadena, CA 91125 USA.
[Irwin, Rossman P., III] Smithsonian Inst, Natl Air & Space Museum, Ctr Earth & Planetary Studies, Washington, DC 20013 USA.
[Collins, Geoffrey C.] Wheaton Coll, Dept Phys & Astron, Norton, MA 02766 USA.
[Howard, Alan D.] Univ Virginia, Dept Environm Sci, Charlottesville, VA 22904 USA.
[Sklar, Leonard S.] San Francisco State Univ, Dept Geosci, San Francisco, CA 94132 USA.
[Moore, Jeffrey M.] NASA, Space Sci Div, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Adamkovics, Mate] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA.
[Baker, Victor R.] Univ Arizona, Dept Hydrol & Water Resources, Tucson, AZ 85721 USA.
RP Burr, DM (reprint author), Univ Tennessee, Dept Earth & Planetary Sci, 1412 Circle Dr, Knoxville, TN 37996 USA.
EM dburr1@utk.edu
RI Lamb, Michael/B-6478-2012; Perron, J. Taylor/D-8983-2012;
OI Perron, J. Taylor/0000-0002-0404-8701; Sklar,
Leonard/0000-0001-9626-733X; Howard, Alan/0000-0002-5423-1600
FU Cassini Data Analysis Program; Outer Planets Research Program;
University of Tennessee
FX Support for Burr, Irwin, Perron, Drummond, and Black was provided by a
Cassini Data Analysis Program grant to Burr. Collins and Sklar were
supported by an Outer Planets Research Program grant to Collins. Moore
and Howard were supported by an Outer Planets Research Program grant to
Moore. We acknowledge support from the University of Tennessee Exhibit,
Performance, and Publication Expense Fund. We thank Tom Farr for
processing the synthetic aperture radar (SAR) images in Figure 4. We
gratefully acknowledge Trent Hare for his Titan ArcGIS project and Randy
Kirk and Alex Hayes for helpful information. We thank the editors for
their assistance in helping us shape this publication appropriately, and
Bob Craddock, Ralph Lorenz, and an anonymous reviewer for providing
useful comments. Most of all, we thank the Cassini and Huygens
spacecraft mission teams for their successful efforts to produce the
data used in this manuscript.
NR 201
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U2 31
PU GEOLOGICAL SOC AMER, INC
PI BOULDER
PA PO BOX 9140, BOULDER, CO 80301-9140 USA
SN 0016-7606
EI 1943-2674
J9 GEOL SOC AM BULL
JI Geol. Soc. Am. Bull.
PD MAR-APR
PY 2013
VL 125
IS 3-4
BP 299
EP 321
DI 10.1130/B30612.1
PG 23
WC Geosciences, Multidisciplinary
SC Geology
GA 130IJ
UT WOS:000317907000003
ER
PT J
AU Scheingross, JS
Minchew, BM
Mackey, BH
Simons, M
Lamb, MP
Hensley, S
AF Scheingross, Joel S.
Minchew, Brent M.
Mackey, Benjamin H.
Simons, Mark
Lamb, Michael P.
Hensley, Scott
TI Fault-zone controls on the spatial distribution of slow-moving
landslides
SO GEOLOGICAL SOCIETY OF AMERICA BULLETIN
LA English
DT Article
ID SAN-ANDREAS-FAULT; OREGON COAST RANGE; CENTRAL CALIFORNIA; THRESHOLD
HILLSLOPES; LANDSCAPE EVOLUTION; SEASONAL MOVEMENT; CREEPING SEGMENT;
ACTIVE EARTHFLOW; BRITISH-COLUMBIA; MASS MOVEMENTS
AB Slow-moving landslides (earthflows) can dominate hillslope sediment flux and landscape erosion in hilly terrain with mechanically weak, fine-grained rock. Controls on the occurrence of slow-moving landslides are poorly constrained and need to be under stood for landscape evolution models, sediment budgets, and infrastructure and hazards planning. Here, we use airborne interferometric synthetic aperture radar (InSAR) and aerial photographs to document 150 previously unidentified active earthflows along the central, creeping portion of the San Andreas fault, California. The earthflows move seasonally in response to winter rainfall, occur on hillslopes at similar to 20%-40% gradients (less than typically associated with rapid, catastrophic landslides), and have similar morphological characteristics to earthflows in different climatic and tectonic settings. Although our data extend up to 10 km from the fault trace, similar to 75% of detected landslides occur within 2 km of the active fault. Topographic, precipitation, and rock type metrics alone are not enough to explain the observed spatial distribution of earthflows. Instead, we hypothesize that earthflows cluster near the creeping San Andreas fault because of a fault-induced zone of reduced bulk-rock strength that increases hillslope susceptibility to failure. In addition, similar lithology, topography, and climate exist north of the creeping section of the fault, yet earthflows there are rare. This may be due to large-magnitude earthquakes episodically triggering coseismic rapid landslides, which preferentially remove weak rock from the fault damage zone. Our analysis suggests that the necessary conditions for earthflow formation in central California include some combination of reduced rock strength, fine-grained sedimentary rock, threshold precipitation and relief, and possibly the absence of large-magnitude earthquakes. These conditions likely hold for earthflow development in other areas, and our work suggests that local variations in rock strength and seismicity, such as those associated with fault zones, need to be taken into account in order to accurately predict earthflow occurrence.
C1 [Scheingross, Joel S.; Mackey, Benjamin H.; Lamb, Michael P.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA.
[Minchew, Brent M.; Simons, Mark] CALTECH, Div Geol & Planetary Sci, Seismol Lab, Pasadena, CA 91125 USA.
[Hensley, Scott] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
RP Scheingross, JS (reprint author), CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA.
EM jscheingross@caltech.edu
RI Lamb, Michael/B-6478-2012; Simons, Mark/N-4397-2015;
OI Simons, Mark/0000-0003-1412-6395; Scheingross, Joel/0000-0002-7220-8084
FU Keck Institute for Space Studies; National Science Foundation
FX We benefited from fruitful discussions with Jean-Philippe Avouac,
Jean-Paul Ampuero, and Piyush Agram. Eric Fielding, Yang Zheng, and
Brian Hawkins helped facilitate Uninhabited Aerial Vehicle Synthetic
Aperture Radar (UAVSAR) data access. The Keck Institute for Space
Studies provided funding for this study through the Advanced Earth
Surface Observation Project. Scheingross was partially supported by a
National Science Foundation Graduate Research Fellowship. We thank three
anonymous reviewers for insightful comments that improved the structure
and clarity of this manuscript.
NR 109
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U1 3
U2 42
PU GEOLOGICAL SOC AMER, INC
PI BOULDER
PA PO BOX 9140, BOULDER, CO 80301-9140 USA
SN 0016-7606
J9 GEOL SOC AM BULL
JI Geol. Soc. Am. Bull.
PD MAR-APR
PY 2013
VL 125
IS 3-4
BP 473
EP 489
DI 10.1130/B30719.1
PG 17
WC Geosciences, Multidisciplinary
SC Geology
GA 130IJ
UT WOS:000317907000013
ER
PT J
AU Gofford, J
Reeves, JN
Tombesi, F
Braito, V
Turner, TJ
Miller, L
Cappi, M
AF Gofford, Jason
Reeves, James N.
Tombesi, Francesco
Braito, Valentina
Turner, T. Jane
Miller, Lance
Cappi, Massimo
TI The Suzaku view of highly ionized outflows in AGN - I. Statistical
detection and global absorber properties
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE line: identification; galaxies: active; galaxies: nuclei; X-rays:
galaxies
ID ACTIVE GALACTIC NUCLEI; X-RAY EXCESS; ULTRA-FAST OUTFLOWS;
RADIATION-MAGNETOHYDRODYNAMIC SIMULATIONS; SHELL ABSORPTION-LINES;
RADIO-QUIET AGNS; GALAXY 3C 445; XMM-NEWTON; BLACK-HOLE; IRON LINE
AB We present the results of a new spectroscopic study of Fe K-band absorption in active galactic nuclei (AGN). Using data obtained from the Suzaku public archive we have performed a statistically driven blind search for Fe XXV He alpha and/or Fe XXVI Ly alpha absorption lines in a large sample of 51 Type 1.0-1.9 AGN. Through extensive Monte Carlo simulations we find that statistically significant absorption is detected at E greater than or similar to 6.7 keV in 20/51 sources at the P-MC = 95 per cent level, which corresponds to similar to 40 per cent of the total sample. In all cases, individual absorption lines are detected independently and simultaneously amongst the two (or three) available X-ray imaging spectrometer detectors, which confirms the robustness of the line detections. The most frequently observed outflow phenomenology consists of two discrete absorption troughs corresponding to Fe XXV He alpha and Fe XXVI Ly alpha at a common velocity shift. From xstar fitting the mean column density and ionization parameter for the Fe K absorption components are log (N-H/cm(-2)) approximate to 23 and log (xi/erg cm s(-1)) approximate to 4.5, respectively. Measured outflow velocities span a continuous range from < 1500 km s(-1) up to similar to 100 000 km s(-1), with mean and median values of similar to 0.1 c and similar to 0.056 c, respectively. The results of this work are consistent with those recently obtained using XMM-Newton and independently provides strong evidence for the existence of very highly ionized circumnuclear material in a significant fraction of both radio-quiet and radio-loud AGN in the local universe.
C1 [Gofford, Jason; Reeves, James N.] Keele Univ, Astrophys Grp, Keele ST5 5BG, Staffs, England.
[Reeves, James N.; Turner, T. Jane] Univ Maryland Baltimore Cty, Dept Phys, Baltimore, MD 21250 USA.
[Tombesi, Francesco] NASA, Xray Astrophys Lab, GSFC, Greenbelt, MD 20771 USA.
[Tombesi, Francesco] NASA, CRESST, GSFC, Greenbelt, MD 20771 USA.
[Tombesi, Francesco] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Braito, Valentina] INAF Osservatorio Astron Brera, I-23807 Merate, Italy.
[Braito, Valentina] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England.
[Miller, Lance] Univ Oxford, Dept Phys, Oxford OX1 3RH, England.
[Cappi, Massimo] INAF IASF Bologna, I-40129 Bologna, Italy.
RP Gofford, J (reprint author), Keele Univ, Astrophys Grp, Keele ST5 5BG, Staffs, England.
EM jag@astro.keele.ac.uk
RI Cappi, Massimo/F-4813-2015; XRAY, SUZAKU/A-1808-2009;
OI Cappi, Massimo/0000-0001-6966-8920; Braito,
Valentina/0000-0002-2629-4989
FU Science and Technology Facilities Council (STFC, UK); NASA [NNX11AJ57G];
ASI [I/009/10/0]; INAF
FX This research has used data obtained from the Suzaku X-ray observatory,
which is a collaborative mission between the Japan Aerospace Exploration
Agency (JAXA, Japan) and the National Aeronautics and Space
Administration (NASA, USA). Data were obtained from the High Energy
Astrophysics Science Archive Research Center (HEASARC) via the Data
Archives and Transmission System (DARTS), which are provided by NASA's
Goddard Space Flight Center and JAXA's Institute of Space and
Aeronautical Science, respectively. Source classifications and
red-shifts were obtained from the NASA/IPAC Extragalactic Database (NED)
and the SIMBAD data base, which are operated by the Jet Propulsion
Laboratory, California Institute of Technology, under contract with the
National Aeronautics and Space Administration, and at the Centre de
Donnees astronomiques (CDS), Strasbourg, France. We would like to thank
the anonymous referee for her/his comments and suggestions which have
helped improved the quality of this manuscript. JG acknowledges support
from the Science and Technology Facilities Council (STFC, UK) in the
form of a funded Ph.D. studentship and would like to thank A. L. Dobson
for offering several useful comments pertaining to the structure and
content of this paper. TJT acknowledges support from NASA grant
NNX11AJ57G. MC acknowledges financial support from ASI contract
I/009/10/0 and INAF contract PRIN-2011.
NR 104
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PI OXFORD
PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND
SN 0035-8711
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD MAR
PY 2013
VL 430
IS 1
BP 60
EP 80
DI 10.1093/mnras/sts481
PG 21
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 135FU
UT WOS:000318274500019
ER
PT J
AU Rocha, M
Peter, AHG
Bullock, JS
Kaplinghat, M
Garrison-Kimmel, S
Onorbe, J
Moustakas, LA
AF Rocha, Miguel
Peter, Annika H. G.
Bullock, James S.
Kaplinghat, Manoj
Garrison-Kimmel, Shea
Onorbe, Jose
Moustakas, Leonidas A.
TI Cosmological simulations with self-interacting dark matter - I.
Constant-density cores and substructure
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE methods: numerical; galaxies: haloes; dark matter
ID EARLY-TYPE GALAXIES; DIGITAL SKY SURVEY; DISPERSION-SUPPORTED GALAXIES;
COMPLETE SPECTROSCOPIC SURVEY; MILKY-WAY SATELLITES; DWARF GALAXIES;
X-RAY; FUNDAMENTAL PLANE; LAMBDA-CDM; LENSING ANALYSIS
AB We use cosmological simulations to study the effects of self-interacting dark matter (SIDM) on the density profiles and substructure counts of dark-matter haloes from the scales of spiral galaxies to galaxy clusters, focusing explicitly on models with cross-sections over dark-matter particle mass sigma/m = 1 and 0.1 cm(2) g(-1). Our simulations rely on a new SIDM N-body algorithm that is derived self-consistently from the Boltzmann equation and that reproduces analytic expectations in controlled numerical experiments. We find that well-resolved SIDM haloes have constant-density cores, with significantly lower central densities than their cold dark matter (CDM) counterparts. In contrast, the subhalo content of SIDM haloes is only modestly reduced compared to CDM, with the suppression greatest for large hosts and small halo-centric distances. Moreover, the large-scale clustering and halo circular velocity functions in SIDM are effectively identical to CDM, meaning that all of the large-scale successes of CDM are equally well matched by SIDM. From our largest cross-section runs, we are able to extract scaling relations for core sizes and central densities over a range of halo sizes and find a strong correlation between the core radius of an SIDM halo and the NFW scale radius of its CDM counterpart. We construct a simple analytic model, based on CDM scaling relations, that captures all aspects of the scaling relations for SIDM haloes. Our results show that halo core densities in sigma/m = 1 cm(2) g(-1) models are too low to match observations of galaxy clusters, low surface brightness spirals (LSBs) and dwarf spheroidal galaxies. However, SIDM with sigma/m similar or equal to 0.1 cm(2) g(-1) appears capable of reproducing reported core sizes and central densities of dwarfs, LSBs and galaxy clusters without the need for velocity dependence. Higher resolution simulations over a wider range of masses will be required to confirm this expectation. We discuss constraints arising from the Bullet cluster observations, measurements of dark-matter density on small scales and subhalo survival requirements, and show that SIDM models with sigma/m similar or equal to 0.1 cm(2) g(-1) similar or equal to 0.2 barn GeV-1 are consistent with all observational constraints.
C1 [Rocha, Miguel; Peter, Annika H. G.; Bullock, James S.; Kaplinghat, Manoj; Garrison-Kimmel, Shea; Onorbe, Jose] Univ Calif Irvine, Dept Phys & Astron, Ctr Cosmol, Irvine, CA 92697 USA.
[Moustakas, Leonidas A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Rocha, M (reprint author), Univ Calif Irvine, Dept Phys & Astron, Ctr Cosmol, Irvine, CA 92697 USA.
EM rocham@uci.edu
RI Peter, Annika/D-3698-2015; Bullock, James/K-1928-2015;
OI Bullock, James/0000-0003-4298-5082; Moustakas,
Leonidas/0000-0003-3030-2360
FU CONACyT; NASA [NNX09AG01G, NNX09AD09G]; Gary McCue Fellowship through
the Center for Cosmology at UC Irvine; NASA at UCI [NNX09AD09G];
National Science Foundation (NSF) at UCI [0855462]; NSF [0855462, NSF
PHY11-25915]; Miller Institute for Basic Research in Science;
Fullbright-MICINN; Perimeter Institute of Theoretical Physics;
Government of Canada through Industry Canada; Province of Ontario
through the Ministry of Economic Development and Innovation; NASA ATFP
FX MR was supported by a CONACyT doctoral Fellowship and NASA grant
NNX09AG01G. AHGP is supported by a Gary McCue Fellowship through the
Center for Cosmology at UC Irvine, NASA Grant No. NNX09AD09G at UCI,
National Science Foundation (NSF) grant 0855462 at UCI and the NSF under
Grant No. NSF PHY11-25915 while visiting the Kavli Institute for
Theoretical Physics. JSB was partially supported by the Miller Institute
for Basic Research in Science during a Visiting Miller Professorship in
the Department of Astronomy at the University of California Berkeley. JO
was supported by a Fullbright-MICINN Post-doctoral Fellowship. MK is
supported by NASA grant NNX09AD09G and NSF grant 0855462. This research
was supported in part by the Perimeter Institute of Theoretical Physics
during a visit by MK. Research at Perimeter Institute is supported by
the Government of Canada through Industry Canada and by the Province of
Ontario through the Ministry of Economic Development and Innovation. The
work of LAM was carried out at Jet Propulsion Laboratory, California
Institute of Technology, under a contract with NASA. LAM acknowledges
NASA ATFP support. Simulations were performed in the Pleiades
supercomputer of the NASA Advanced Supercomputing (NAS) Division, and
the Kraken supercomputer of the National Institute for Computational
Sciences (NICS) through an XSEDE allocation.
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JI Mon. Not. Roy. Astron. Soc.
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SC Astronomy & Astrophysics
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ER
PT J
AU Espinoza, CM
Guillemot, L
Celik, O
Weltevrede, P
Stappers, BW
Smith, DA
Kerr, M
Zavlin, VE
Cognard, I
Eatough, RP
Freire, PCC
Janssen, GH
Camilo, F
Desvignes, G
Hewitt, JW
Hou, X
Johnston, S
Keith, M
Kramer, M
Lyne, A
Manchester, RN
Ransom, SM
Ray, PS
Shannon, R
Theureau, G
Webb, N
AF Espinoza, C. M.
Guillemot, L.
Celik, Oe
Weltevrede, P.
Stappers, B. W.
Smith, D. A.
Kerr, M.
Zavlin, V. E.
Cognard, I.
Eatough, R. P.
Freire, P. C. C.
Janssen, G. H.
Camilo, F.
Desvignes, G.
Hewitt, J. W.
Hou, X.
Johnston, S.
Keith, M.
Kramer, M.
Lyne, A.
Manchester, R. N.
Ransom, S. M.
Ray, P. S.
Shannon, R.
Theureau, G.
Webb, N.
TI Six millisecond pulsars detected by the Fermi Large Area Telescope and
the radio/gamma-ray connection of millisecond pulsars
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE pulsars: general; gamma-rays: general; X-rays: general
ID NEUTRON-STAR ATMOSPHERES; NANCAY RADIO TELESCOPE; PULSED GAMMA-RAYS; PSR
J2051-0827; LIGHT CURVES; GIANT PULSES; POLARIZATION OBSERVATIONS;
TIMING OBSERVATIONS; MAGNETIC-FIELDS; BINARY-SYSTEM
AB We report on the discovery of gamma-ray pulsations from five millisecond pulsars (MSPs) using the Fermi Large Area Telescope (LAT) and timing ephemerides provided by various radio observatories. We also present confirmation of the gamma-ray pulsations from a sixth source, PSR J2051-0827. Five of these six MSPs are in binary systems: PSRs J1713+0747, J1741+1351, J1600-3053 and the two black widow binary pulsars PSRs J0610-2100 and J2051-0827. The only isolated MSP is the nearby PSR J1024-0719, which is also known to emit X-rays. We present X-ray observations in the direction of PSRs J1600-3053 and J2051-0827. While PSR J2051-0827 is firmly detected, we can only give upper limits for the X-ray flux of PSR J1600-3053. There are no dedicated X-ray observations available for the other three objects.
The MSPs mentioned above, together with most of the MSPs detected by Fermi, are used to put together a sample of 30 gamma-ray MSPs. This sample is used to study the morphology and phase connection of radio and gamma-ray pulse profiles. We show that MSPs with pulsed gamma-ray emission which is phase-aligned with the radio emission present the steepest radio spectra and the largest magnetic fields at the light cylinder among all MSPs. Also, we observe a trend towards very low, or undetectable, radio linear polarization levels. These properties could be attributed to caustic radio emission produced at a range of different altitudes in the magnetosphere. We note that most of these characteristics are also observed in the Crab pulsar, the only other radio pulsar known to exhibit phase-aligned radio and gamma-ray emission.
C1 [Espinoza, C. M.; Weltevrede, P.; Stappers, B. W.; Janssen, G. H.; Kramer, M.; Lyne, A.] Univ Manchester, Sch Phys & Astron, Jodrell Bank Ctr Astrophys, Manchester M13 9PL, Lancs, England.
[Guillemot, L.; Eatough, R. P.; Freire, P. C. C.; Desvignes, G.; Kramer, M.] Max Planck Inst Radioastron, D-53121 Bonn, Germany.
[Celik, Oe; Hewitt, J. W.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Celik, Oe] CRESST, Greenbelt, MD 20771 USA.
[Celik, Oe] Univ Maryland Baltimore Cty, Dept Phys, Baltimore, MD 21250 USA.
[Celik, Oe] Univ Maryland Baltimore Cty, Ctr Space Sci & Technol, Baltimore, MD 21250 USA.
[Smith, D. A.; Hou, X.] Univ Bordeaux 1, CNRS, IN2P3, Ctr Etud Nucl Bordeaux Gradignan, F-33175 Gradignan, France.
[Kerr, M.] Stanford Univ, WW Hansen Expt Phys Lab, Kavli Inst Particle Astrophys & Cosmol, Dept Phys, Stanford, CA 94305 USA.
[Kerr, M.] Stanford Univ, SLAC Natl Accelerator Lab, Stanford, CA 94305 USA.
[Zavlin, V. E.] NASA, Space Sci Lab, Marshall Space Flight Ctr, Huntsville, AL 35805 USA.
[Zavlin, V. E.] USRA Sci & Technol Inst, Huntsville, AL 35805 USA.
[Cognard, I.; Desvignes, G.; Theureau, G.] CNRS, UMR 6115, LPCE, F-45071 Orleans 02, France.
[Cognard, I.; Desvignes, G.; Theureau, G.] CNRS, INSU, Observ Paris, Stn Radioastron Nancay, F-18330 Nancay, France.
[Camilo, F.] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA.
[Camilo, F.] Arecibo Observ, Arecibo, PR 00612 USA.
[Johnston, S.; Keith, M.; Manchester, R. N.; Shannon, R.] Australia Telescope Natl Facil, CSIRO Astron & Space Sci, Epping, NSW 1710, Australia.
[Ransom, S. M.] NRAO, Charlottesville, VA 22903 USA.
[Ray, P. S.] USN, Space Sci Div, Res Lab, Washington, DC 20375 USA.
[Webb, N.] CNRS, IRAP, F-31028 Toulouse 4, France.
[Webb, N.] Univ Toulouse, UPS, OMP, GAHEC,IRAP, Toulouse, France.
RP Espinoza, CM (reprint author), Univ Manchester, Sch Phys & Astron, Jodrell Bank Ctr Astrophys, Manchester M13 9PL, Lancs, England.
EM cme@jb.man.ac.uk
OI Shannon, Ryan/0000-0002-7285-6348; Ransom, Scott/0000-0001-5799-9714;
Ray, Paul/0000-0002-5297-5278
FU Science and Technology Facilities Council of the United Kingdom;
Commonwealth Government; National Science Foundation [AST-1100968]
FX The Nancay Radio Observatory is operated by the Paris Observatory,
associated with the French Centre National de la Recherche Scientifique
(CNRS). The Lovell Telescope is owned and operated by the University of
Manchester as part of the Jodrell Bank Centre for Astrophysics, with
support from the Science and Technology Facilities Council of the United
Kingdom. The Westerbork Synthesis Radio Telescope is operated by the
Netherlands Foundation for Radio Astronomy, ASTRON. The Parkes Radio
Telescope is part of the Australia Telescope, which is funded by the
Commonwealth Government for operation as a National Facility managed by
CSIRO. We thank our colleagues for their assistance with the radio
timing observations. The Arecibo Observatory is operated by SRI
International under a cooperative agreement with the National Science
Foundation (AST-1100968), and in alliance with Ana G. Mendez-Universidad
Metropolitana and the Universities Space Research Association.
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SC Astronomy & Astrophysics
GA 135FU
UT WOS:000318274500051
ER
PT J
AU Miller, L
Heymans, C
Kitching, TD
van Waerbeke, L
Erben, T
Hildebrandt, H
Hoekstra, H
Mellier, Y
Rowe, BTP
Coupon, J
Dietrich, JP
Fu, L
Harnois-Deraps, J
Hudson, MJ
Kilbinger, M
Kuijken, K
Schrabback, T
Semboloni, E
Vafaei, S
Velander, M
AF Miller, L.
Heymans, C.
Kitching, T. D.
van Waerbeke, L.
Erben, T.
Hildebrandt, H.
Hoekstra, H.
Mellier, Y.
Rowe, B. T. P.
Coupon, J.
Dietrich, J. P.
Fu, L.
Harnois-Deraps, J.
Hudson, M. J.
Kilbinger, M.
Kuijken, K.
Schrabback, T.
Semboloni, E.
Vafaei, S.
Velander, M.
TI Bayesian galaxy shape measurement for weak lensing surveys - III.
Application to the Canada-France-Hawaii Telescope Lensing Survey
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE gravitational lensing: weak; methods: data analysis; methods:
statistical; cosmology: observations
ID DIGITAL SKY SURVEY; ON SPIRAL GALAXIES; 3-DIMENSIONAL DISTRIBUTION;
SURFACE PHOTOMETRY; IMAGE-ANALYSIS; DARK-MATTER; NOISE BIAS; SHEAR;
FIELD; CALIBRATION
AB A likelihood-based method for measuring weak gravitational lensing shear in deep galaxy surveys is described and applied to the Canada-France-Hawaii Telescope (CFHT) Lensing Survey (CFHTLenS). CFHTLenS comprises 154 deg(2) of multi-colour optical data from the CFHT Legacy Survey, with lensing measurements being made in the i' band to a depth i(AB)' < 24.7, for galaxies with signal-to-noise ratio nu(SN) greater than or similar to 10. The method is based on the lensfit algorithm described in earlier papers, but here we describe a full analysis pipeline that takes into account the properties of real surveys. The method creates pixel-based models of the varying point spread function (PSF) in individual image exposures. It fits PSF-convolved two-component (disc plus bulge) models to measure the ellipticity of each galaxy, with Bayesian marginalization over model nuisance parameters of galaxy position, size, brightness and bulge fraction. The method allows optimal joint measurement of multiple, dithered image exposures, taking into account imaging distortion and the alignment of the multiple measurements. We discuss the effects of noise bias on the likelihood distribution of galaxy ellipticity. Two sets of image simulations that mirror the observed properties of CFHTLenS have been created to establish the method's accuracy and to derive an empirical correction for the effects of noise bias.
C1 [Miller, L.; Velander, M.] Univ Oxford, Dept Phys, Oxford OX1 3RH, England.
[Heymans, C.; Kitching, T. D.] Univ Edinburgh, Royal Observ, Scottish Univ Phys Alliance, Inst Astron, Edinburgh EH9 3HJ, Midlothian, Scotland.
[van Waerbeke, L.; Hildebrandt, H.; Vafaei, S.] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada.
[Erben, T.; Hildebrandt, H.; Schrabback, T.] Univ Bonn, Argelander Inst Astron, D-53121 Bonn, Germany.
[Hoekstra, H.; Kuijken, K.; Schrabback, T.; Semboloni, E.; Velander, M.] Leiden Univ, Leiden Observ, NL-2333 CA Leiden, Netherlands.
[Hoekstra, H.] Univ Victoria, Dept Phys & Astron, Victoria, BC V8P 5C2, Canada.
[Mellier, Y.; Kilbinger, M.] Univ Paris 06, Inst Astrophys Paris, F-75014 Paris, France.
[Rowe, B. T. P.] UCL, Dept Phys & Astron, London WC1E 6BT, England.
[Rowe, B. T. P.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Rowe, B. T. P.] CALTECH, Pasadena, CA 91125 USA.
[Coupon, J.] Acad Sinica, Inst Astron & Astrophys, Taipei 10617, Taiwan.
[Dietrich, J. P.] Univ Michigan, Dept Phys, Ann Arbor, MI 48109 USA.
[Fu, L.] Shanghai Normal Univ, Key Lab Astrophys, Shanghai 200234, Peoples R China.
[Harnois-Deraps, J.] Univ Toronto, Canadian Inst Theoret Astrophys, Toronto, ON M5S 3H8, Canada.
[Harnois-Deraps, J.] Univ Toronto, Dept Phys, Toronto, ON M5S 1A7, Canada.
[Hudson, M. J.] Univ Waterloo, Dept Phys & Astron, Waterloo, ON N2L 3G1, Canada.
[Hudson, M. J.] Perimeter Inst Theoret Phys, Waterloo, ON N2L 1Y5, Canada.
[Kilbinger, M.] CEA Saclay, Serv Astrophys SAp, F-91191 Gif Sur Yvette, France.
[Kilbinger, M.] Excellence Cluster Universe, D-85748 Garching, Germany.
[Kilbinger, M.] Univ Munich, Univ Sternwarte, D-81679 Munich, Germany.
[Schrabback, T.] Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, Stanford, CA 94305 USA.
RP Miller, L (reprint author), Univ Oxford, Dept Phys, Keble Rd, Oxford OX1 3RH, England.
EM l.miller1@physics.ox.ac.uk
RI Hudson, Michael/H-3238-2012;
OI Hudson, Michael/0000-0002-1437-3786; Dietrich, Jorg/0000-0002-8134-9591;
Rowe, Barnaby/0000-0002-7042-9174; Kilbinger,
Martin/0000-0001-9513-7138; Hoekstra, Henk/0000-0002-0641-3231
FU Canadian Space Agency; European Research Council under the EC [240185];
Royal Society; Natural Sciences and Engineering Research Council of
Canada (NSERC); Canadian Institute for Advanced Research (CIfAR,
Cosmology and Gravity program); Deutsche Forschungsgemeinschaft [ER
327/3-1]; Transregional Collaborative Research Centre [TR 33 - 'The Dark
Universe']; Marie Curie IOF [252760]; CITA; Marie Curie IRG grant
[230924]; Netherlands Organization for Scientific Research (NWO)
[639.042.814]; European Research Council under the EC FP7 grant
[279396]; CNRS/INSU (Institut National des Sciences de l'Univers);
Programme National Galaxies et Cosmologie (PNCG); NSF [AST 0807304,
AST-0444059-001]; NSFC [11103012, 10878003]; Innovation Program
[12ZZ134]; Chen Guang project of SMEC [10CG46]; STCSM [11290706600];
Pujiang Program [12PJ1406700]; SAO [GO0-11147A]; NWO; Netherlands
Organization for Scientific Research (NWO); Beecroft Institute for
Particle Astrophysics and Cosmology; Canada Foundation for Innovation
under Compute Canada; Government of Ontario; Ontario Research Fund -
Research Excellence; University of Toronto
FX This work is based on observations obtained with MegaPrime/MegaCam, a
joint project of CFHT and CEA/DAPNIA, at the CFHT which is operated by
the National Research Council (NRC) of Canada, the Institut National des
Sciences de l'Univers of the Centre National de la Recherche
Scientifique (CNRS) of France, and the University of Hawaii. This
research used the facilities of the Canadian Astronomy Data Centre
operated by the National Research Council of Canada with the support of
the Canadian Space Agency. We thank the CFHT staff for successfully
conducting the CFHTLS observations and in particular Jean-Charles
Cuillandre and Eugene Magnier for the continuous improvement of the
instrument calibration and the Elixir detrended data that we used. We
also thank TERAPIX for the individual exposures quality assessment and
validation during the CFHTLS data acquisition period, and Emmanuel
Bertin for developing some of the software used in this study. CFHTLenS
data processing was made possible thanks to significant computing
support from the NSERC Research Tools and Instruments grant program, and
to HPC specialist Ovidiu Toader.; CH acknowledges support from the
European Research Council under the EC FP7 grant number 240185. TDK
acknowledges support from a Royal Society University Research
Fellowship. LVW acknowledges support from the Natural Sciences and
Engineering Research Council of Canada (NSERC) and the Canadian
Institute for Advanced Research (CIfAR, Cosmology and Gravity program).
TE is supported by the Deutsche Forschungsgemeinschaft through project
ER 327/3-1 and the Transregional Collaborative Research Centre TR 33 -
'The Dark Universe'. H. Hildebrandt is supported by the Marie Curie IOF
252760 and by a CITA National Fellowship. H. Hoekstra acknowledges
support from Marie Curie IRG grant 230924, the Netherlands Organization
for Scientific Research (NWO) grant number 639.042.814 and from the
European Research Council under the EC FP7 grant number 279396. YM
acknowledges support from CNRS/INSU (Institut National des Sciences de
l'Univers) and the Programme National Galaxies et Cosmologie (PNCG). JPD
was supported by NSF grant AST 0807304. LF acknowledges support from
NSFC grants 11103012 and 10878003, Innovation Program 12ZZ134 and Chen
Guang project 10CG46 of SMEC, STCSM grant 11290706600 and Pujiang
Program 12PJ1406700. MJH acknowledges support from the Natural Sciences
and Engineering Research Council of Canada (NSERC). TS acknowledges
support from NSF through grant AST-0444059-001, SAO through grant
GO0-11147A, and NWO. MV acknowledges support from the Netherlands
Organization for Scientific Research (NWO) and from the Beecroft
Institute for Particle Astrophysics and Cosmology.; The N-body
simulations used in this analysis were performed on the TCS
supercomputer at the SciNet HPC Consortium. SciNet is funded by: the
Canada Foundation for Innovation under the auspices of Compute Canada;
the Government of Ontario; Ontario Research Fund - Research Excellence;
and the University of Toronto. We thank Sree Balan, Sarah Bridle and
Emmanuel Bertin for the simulation code used in this analysis.
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PT J
AU Jeffery, CS
Ramsay, G
Naslim, N
Carrera, R
Greiss, S
Barclay, T
Karjalainen, R
Brooks, A
Hakala, P
AF Jeffery, C. S.
Ramsay, G.
Naslim, N.
Carrera, R.
Greiss, S.
Barclay, T.
Karjalainen, R.
Brooks, A.
Hakala, P.
TI KIC 10449976: discovery of an extreme helium subdwarf in the Kepler
field
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE stars: abundances; stars: chemically peculiar; stars: individual: KIC
10449976; subdwarfs
ID HYDROGEN-DEFICIENT STARS; SIGMA-ORIONIS-E; B-STARS; VARIABLE-STARS;
HORIZONTAL-BRANCH; SPECTRAL-ANALYSIS; VARIABILITY; PARAMETERS;
PULSATION; CATALOG
AB Optical spectroscopy of the blue star KIC 10449976 shows that it is an extremely helium-rich subdwarf with effective temperature T-eff = 40 000 +/- 300 K and surface gravity log g = 5.3 +/- 0.1. Radial-velocity measurements over a 5 d time-scale show an upper variability limit of approximate to 50 +/- 20 km s(-1). Kepler photometry of KIC 10449976 in both long and short cadence modes shows evidence for a periodic modulation on a time-scale of approximate to 3.9 d. We have examined the possibility that this modulation is not astrophysical but conclude that it is most likely real. We discuss whether the modulation could be caused by a low-mass companion, by stellar pulsations or by spots. The identification of any one of these as cause has important consequences for understanding the origin of helium-rich subdwarfs.
C1 [Jeffery, C. S.; Ramsay, G.; Naslim, N.; Brooks, A.] Armagh Observ, Armagh BT61 9DG, North Ireland.
[Carrera, R.] Inst Astrofis Canarias, E-3200 Tenerife, Spain.
[Carrera, R.] Univ La Laguna, Dept Astrofis, E-38205 Tenerife, Spain.
[Greiss, S.] Univ Warwick, Dept Phys, Coventry CV4 7AL, W Midlands, England.
[Barclay, T.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Barclay, T.] Bay Area Environm Res Inst Inc, Sonoma, CA 95476 USA.
[Karjalainen, R.] Isaac Newton Grp Telescopes, E-38700 Santa Cruz De La Palma, Canary Islands, Spain.
[Brooks, A.] Univ Coll London, Mullard Space Sci Lab, Dorking RH5 6NT, Surrey, England.
[Hakala, P.] Univ Turku, Finnish Ctr Astron ESO FINCA, FI-21500 Piikkio, Finland.
RP Jeffery, CS (reprint author), Armagh Observ, Coll Hill, Armagh BT61 9DG, North Ireland.
EM csj@arm.ac.uk
RI Carrera, Ricardo/K-8760-2014;
OI Carrera, Ricardo/0000-0001-6143-8151; Jeffery, C.
Simon/0000-0003-1759-0302
FU Northern Ireland Department of Culture Arts and Leisure; NASA Science
Mission Directorate; NASA [NAS5-26555]; NASA Office of Space Science
[NNX09AF08G]
FX The Armagh Observatory is supported by a grant from the Northern Ireland
Department of Culture Arts and Leisure. The INT and WHT are operated on
the island of La Palma by the Isaac Newton Group in the Spanish
Observatorio del Roque de los Muchachos of the Instituto de Astrofsica
de Canarias. We thank the staff for their support. This paper includes
data collected by the Kepler mission. Funding for the Kepler mission is
provided by the NASA Science Mission Directorate. Some of the data
presented in this paper were obtained from the Mikulski Archive for
Space Telescopes (MAST). STScI is operated by the Association of
Universities for Research in Astronomy, Inc., under NASA contract
NAS5-26555. Support for MAST for non-HST data is provided by the NASA
Office of Space Science via grant NNX09AF08G and by other grants and
contracts.
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ER
PT J
AU Hildebrandt, H
van Waerbeke, L
Scott, D
Bethermin, M
Bock, J
Clements, D
Conley, A
Cooray, A
Dunlop, JS
Eales, S
Erben, T
Farrah, D
Franceschini, A
Glenn, J
Halpern, M
Heinis, S
Ivison, RJ
Marsden, G
Oliver, SJ
Page, MJ
Perez-Fournon, I
Smith, AJ
Rowan-Robinson, M
Valtchanov, I
van der Burg, RFJ
Vieira, JD
Viero, M
Wang, L
AF Hildebrandt, H.
van Waerbeke, L.
Scott, D.
Bethermin, M.
Bock, J.
Clements, D.
Conley, A.
Cooray, A.
Dunlop, J. S.
Eales, S.
Erben, T.
Farrah, D.
Franceschini, A.
Glenn, J.
Halpern, M.
Heinis, S.
Ivison, R. J.
Marsden, G.
Oliver, S. J.
Page, M. J.
Perez-Fournon, I.
Smith, A. J.
Rowan-Robinson, M.
Valtchanov, I.
van der Burg, R. F. J.
Vieira, J. D.
Viero, M.
Wang, L.
TI Inferring the mass of submillimetre galaxies by exploiting their
gravitational magnification of background galaxies
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE gravitational lensing: weak; galaxies: high-redshift; submillimetre:
galaxies
ID LYMAN-BREAK GALAXIES; DARK-MATTER HALOS; STAR-FORMING GALAXIES; COSMIC
MAGNIFICATION; EXTRAGALACTIC SURVEY; CROSS-CORRELATION; MU-M; HERMES;
EVOLUTION; NUMBER
AB Dust emission at submillimetre wavelengths allows us to trace the early phases of star formation in the Universe. In order to understand the physical processes involved in this mode of star formation, it is essential to gain knowledge about the dark matter structures - most importantly their masses - that submillimetre galaxies live in. Here we use the magnification effect of gravitational lensing to determine the average mass and dust content of submillimetre galaxies with 250 mu m flux densities of S-250 > 15 mJy selected using data from the Herschel Multi-tiered Extragalactic Survey. The positions of hundreds of submillimetre foreground lenses are cross-correlated with the positions of background Lyman-break galaxies at z similar to 3-5 selected using optical data from the Canada-France-Hawaii Telescope Legacy Survey. We detect a cross-correlation signal at the 7 sigma level over a sky area of 1 deg(2), with similar to 80 per cent of this signal being due to magnification, whereas the remaining similar to 20 per cent comes from dust extinction. Adopting some simple assumptions for the dark matter and dust profiles and the redshift distribution enables us to estimate the average mass of the haloes hosting the submillimetre galaxies to be log(10)[M-200/M-circle dot] = 13.17(-0.08)(+0.05)(stat.) and their average dust mass fraction (at radii of > 10 kpc) to be M-dust/M-200 approximate to 6 x 10(-5). This supports the picture that submillimetre galaxies are dusty, forming stars at a high rate, reside in massive group-sized haloes and are a crucial phase in the assembly and evolution of structure in the Universe.
C1 [Hildebrandt, H.; van Waerbeke, L.; Scott, D.; Halpern, M.; Marsden, G.] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada.
[Hildebrandt, H.; Erben, T.] Argelander Inst Astron, D-53121 Bonn, Germany.
[Bethermin, M.] Univ Paris Diderot, CNRS, CEA DSM Irfu, Lab AIM Paris Saclay,CE Saclay, F-91191 Gif Sur Yvette, France.
[Bethermin, M.] Univ Paris 11, Inst Astrophys Spatiale, F-91405 Orsay, France.
[Bethermin, M.] CNRS, UMR 8617, F-91405 Orsay, France.
[Bock, J.; Cooray, A.; Vieira, J. D.; Viero, M.] CALTECH, Pasadena, CA 91125 USA.
[Bock, J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Clements, D.; Rowan-Robinson, M.] Univ London Imperial Coll Sci Technol & Med, Astrophys Grp, Blackett Lab, London SW7 2AZ, England.
[Conley, A.; Glenn, J.] Univ Colorado, Dept Astrophys & Planetary Sci, Boulder, CO 80309 USA.
[Cooray, A.] Univ Calif Irvine, Dept Phys & Astron, Irvine, CA 92697 USA.
[Dunlop, J. S.] Univ Edinburgh, SUPA, Inst Astron, Royal Observ, Edinburgh EH9 3HJ, Midlothian, Scotland.
[Eales, S.] Cardiff Univ, Cardiff Sch Phys & Astron, Cardiff CF24 3AA, S Glam, Wales.
[Farrah, D.] Virginia Tech, Dept Phys, Blacksburg, VA 24061 USA.
[Franceschini, A.] Univ Padua, Dipartimento Astron, I-35122 Padua, Italy.
[Glenn, J.] Univ Colorado, Ctr Astrophys & Space Astron, Boulder, CO 80309 USA.
[Heinis, S.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA.
[Ivison, R. J.] Univ Edinburgh, Inst Astron, Royal Observ, Edinburgh EH9 3HJ, Midlothian, Scotland.
[Ivison, R. J.] Royal Observ, UK Astron Technol Ctr, Edinburgh EH9 3HJ, Midlothian, Scotland.
[Oliver, S. J.; Smith, A. J.; Wang, L.] Univ Sussex, Ctr Astron, Dept Phys & Astron, Brighton BN1 9QH, E Sussex, England.
[Page, M. J.] Univ Coll London, Mullard Space Sci Lab, Dorking RH5 6NT, Surrey, England.
[Perez-Fournon, I.] Inst Astrofis Canarias, E-38200 San Cristobal la Laguna, Tenerife, Spain.
[Perez-Fournon, I.] Univ La Laguna, Dept Astrofis, E-38206 Tenerife, Spain.
[Valtchanov, I.] ESA, Herschel Sci Ctr, European Space Astron Ctr, E-28691 Villanueva De La Canada, Spain.
[van der Burg, R. F. J.] Leiden Univ, Leiden Observ, NL-2333 CA Leiden, Netherlands.
RP Hildebrandt, H (reprint author), Univ British Columbia, Dept Phys & Astron, 6224 Agr Rd, Vancouver, BC V6T 1Z1, Canada.
EM hendrikhildebrandt@gmail.com
RI Ivison, R./G-4450-2011;
OI Ivison, R./0000-0001-5118-1313; Scott, Douglas/0000-0002-6878-9840;
Bethermin, Matthieu/0000-0002-3915-2015
FU CSA (Canada); NAOC (China); CEA (France); CNES (France); CNRS (France);
ASI (Italy); MCINN (Spain); SNSB (Sweden); STFC (UK); UKSA (UK); NASA
(USA); Marie Curie IOF [252760]; CITA National Fellowship; DFG [Hi
1495/2-1]; NSERC; CIfAR; CSA; Deutsche Forschungsgemeinschaft [ER
327/3-1]; Transregional Collaborative Research Centre - 'The Dark
Universe' [TR 33]; Netherlands Organisation for Scientic Research
[639.042.814]
FX SPIRE has been developed by a consortium of institutes led by Cardiff
University (UK) and including Univ. Lethbridge (Canada); NAOC (China);
CEA, LAM (France); IFSI, Univ. Padua (Italy); IAC (Spain); Stockholm
Observatory (Sweden); Imperial College London, RAL, UCL-MSSL, UKATC,
Univ. Sussex (UK) and Caltech/JPL, IPAC, Univ. Colorado (USA). This
development has been supported by national funding agencies: CSA
(Canada); NAOC (China); CEA, CNES, CNRS (France); ASI (Italy); MCINN
(Spain); SNSB (Sweden); STFC, UKSA (UK) and NASA (USA).; HH is supported
by the Marie Curie IOF 252760, a CITA National Fellowship and the DFG
grant Hi 1495/2-1. LvW is supported by NSERC and CIfAR. DS acknowledges
support by NSERC and CSA. TE is supported by the Deutsche
Forschungsgemeinschaft through project ER 327/3-1 and the Transregional
Collaborative Research Centre TR 33 - 'The Dark Universe'. RFJvdB
acknowledges support from the Netherlands Organisation for Scientic
Research grant number 639.042.814.
NR 48
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PI OXFORD
PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND
SN 0035-8711
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD MAR
PY 2013
VL 429
IS 4
BP 3230
EP 3237
DI 10.1093/mnras/sts585
PG 8
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 135FD
UT WOS:000318272600037
ER
PT J
AU Badenes, C
van Kerkwijk, MH
Kilic, M
Bickerton, SJ
Mazeh, T
Mullally, F
Tal-Or, L
Thompson, SE
AF Badenes, Carles
van Kerkwijk, Marten H.
Kilic, Mukremin
Bickerton, Steven J.
Mazeh, Tsevi
Mullally, Fergal
Tal-Or, Lev
Thompson, Susan E.
TI SDSS 1355+0856: a detached white dwarf plus M star binary in the period
gap discovered by the SWARMS survey
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE binaries: close; binaries: spectroscopic; stars: individual: SDSS
1355+0856; white dwarfs
ID COMMON-ENVELOPE BINARIES; MASSIVE NEUTRON-STAR; DEEP SKY SURVEY;
CATACLYSMIC VARIABLES; MAGNETIC BRAKING; RADIAL-VELOCITY; ORBITAL
PERIOD; EVOLUTION; COMPANION; CALIBRATION
AB SDSS J135523.92 + 085645.4 (SDSS 1355+0856) was identified as a hot white dwarf with a companion from time-resolved Sloan Digital Sky Survey spectroscopy as part of the ongoing Sloan White Dwarf Radial velocity data Mining Survey survey. Follow-up observations with the Astrophysical Research Consortium 3.5 m telescope and the Multiple Mirror Telescope revealed weak emission lines in the central cores of the Balmer absorption lines during some phases of the orbit, but no line emission during other phases. This can be explained if SDSS 1355+0856 is a detached white dwarf + M dwarf binary similar to GD 448, where one of the hemispheres of the low-mass companion is irradiated by the proximity of the hot white dwarf. Based on the available data, we derive an orbital period of 0.114 38 +/- 0.000 06 d, a primary mass of 0.46 +/- 0.01 M-circle dot, a secondary mass between 0.083 and 0.097 M-circle dot, and an orbital inclination larger than 57 degrees. This makes SDSS 1355+0856 one of the shortest period post-common envelope white dwarf + M dwarf binaries, and the record holder for the lowest mass stellar companion, which has interesting implications for our understanding of common envelope evolution and the phenomenology of cataclysmic variables. The short cooling time of the WD (25 Myr) implies that the system emerged from the common envelope phase with an orbital period very similar to what we observe today, and was born in the period gap of cataclysmic variables.
C1 [Badenes, Carles] Univ Pittsburgh, Dept Phys & Astron, Pittsburgh, PA 15260 USA.
[Badenes, Carles] Univ Pittsburgh, Dept Phys & Astron, Pittsburgh Particle Phys Astrophys & Cosmol Ctr P, Pittsburgh, PA 15260 USA.
[van Kerkwijk, Marten H.] Univ Toronto, Dept Astron & Astrophys, Toronto, ON M5S 3H4, Canada.
[Kilic, Mukremin] Univ Oklahoma, Homer L Dodge Dept Phys & Astron, Norman, OK 73019 USA.
[Bickerton, Steven J.] Univ Tokyo, IPMU, Chiba 2778582, Japan.
[Mazeh, Tsevi; Tal-Or, Lev] Tel Aviv Univ, Sch Phys & Astron, IL-69978 Tel Aviv, Israel.
[Mullally, Fergal; Thompson, Susan E.] NASA, SETI Inst, Ames Res Ctr, Moffett Field, CA 94035 USA.
RP Badenes, C (reprint author), Univ Pittsburgh, Dept Phys & Astron, 3941 OHara St, Pittsburgh, PA 15260 USA.
EM badenes@pitt.edu
FU Alfred P. Sloan Foundation; National Science Foundation; US Department
of Energy; National Aeronautics and Space Administration; Japanese
Monbukagakusho; Max Planck Society; Higher Education Funding Council for
England; American Museum of Natural History; Astrophysical Institute
Potsdam; University of Basel; University of Cambridge; Case Western
Reserve University; University of Chicago; Drexel University; Fermilab;
Institute for Advanced Study; Japan Participation Group; Johns Hopkins
University; Joint Institute for Nuclear Astrophysics; Kavli Institute
for Particle Astrophysics and Cosmology; Korean Scientist Group; Chinese
Academy of Sciences (LAMOST); Los Alamos National Laboratory;
Max-Planck-Institute for Astronomy (MPIA); Max-Planck-Institute for
Astrophysics (MPA); New Mexico State University; Ohio State University;
University of Pittsburgh; University of Portsmouth; Princeton
University; United States Naval Observatory; University of Washington
FX Funding for the SDSS and SDSS-II has been provided by the Alfred P.
Sloan Foundation, the Participating Institutions, the National Science
Foundation, the US Department of Energy, the National Aeronautics and
Space Administration, the Japanese Monbukagakusho, the Max Planck
Society and the Higher Education Funding Council for England. The SDSS
website is http://www.sdss.org/. The SDSS is managed by the
Astrophysical Research Consortium for the Participating Institutions.
The Participating Institutions are the American Museum of Natural
History, Astrophysical Institute Potsdam, University of Basel,
University of Cambridge, Case Western Reserve University, University of
Chicago, Drexel University, Fermilab, the Institute for Advanced Study,
the Japan Participation Group, Johns Hopkins University, the Joint
Institute for Nuclear Astrophysics, the Kavli Institute for Particle
Astrophysics and Cosmology, the Korean Scientist Group, the Chinese
Academy of Sciences (LAMOST), Los Alamos National Laboratory, the
Max-Planck-Institute for Astronomy (MPIA), the Max-Planck-Institute for
Astrophysics (MPA), New Mexico State University, Ohio State University,
University of Pittsburgh, University of Portsmouth, Princeton
University, the United States Naval Observatory and the University of
Washington.
NR 52
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PI OXFORD
PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND
SN 0035-8711
EI 1365-2966
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD MAR
PY 2013
VL 429
IS 4
BP 3596
EP 3603
DI 10.1093/mnras/sts646
PG 8
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 135FD
UT WOS:000318272600069
ER
PT J
AU Miyatake, H
Nishizawa, AJ
Takada, M
Mandelbaum, R
Mineo, S
Aihara, H
Spergel, DN
Bickerton, SJ
Bond, JR
Gralla, M
Hajian, A
Hilton, M
Hincks, AD
Hughes, JP
Infante, L
Lin, YT
Lupton, RH
Marriage, TA
Marsden, D
Menanteau, F
Miyazaki, S
Moodley, K
Niemack, MD
Oguri, M
Price, PA
Reese, ED
Sifon, C
Wollack, EJ
Yasuda, N
AF Miyatake, Hironao
Nishizawa, Atsushi J.
Takada, Masahiro
Mandelbaum, Rachel
Mineo, Sogo
Aihara, Hiroaki
Spergel, David N.
Bickerton, Steven J.
Bond, J. Richard
Gralla, Megan
Hajian, Amir
Hilton, Matt
Hincks, Adam D.
Hughes, John P.
Infante, Leopoldo
Lin, Yen-Ting
Lupton, Robert H.
Marriage, Tobias A.
Marsden, Danica
Menanteau, Felipe
Miyazaki, Satoshi
Moodley, Kavilan
Niemack, Michael D.
Oguri, Masamune
Price, Paul A.
Reese, Erik D.
Sifon, Cristobal
Wollack, Edward J.
Yasuda, Naoki
TI Subaru weak lensing measurement of a z=0.81 cluster discovered by the
Atacama Cosmology Telescope Survey
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE gravitational lensing: weak; galaxies: clusters: individual: ACT-CL
J0022.2-0036; cosmology: observation
ID DIGITAL SKY SURVEY; SOUTH-POLE TELESCOPE; OSCILLATION SPECTROSCOPIC
SURVEY; STEEP MASS PROFILE; DARK-MATTER HALOS; GALAXY CLUSTERS;
SDSS-III; PHOTOMETRIC REDSHIFTS; IMAGE SUBTRACTION; SUPRIME-CAM
AB We present a Subaru weak lensing measurement of ACT-CL J0022.2-0036, one of the most luminous, high-redshift (z = 0.81) Sunyaev-Zel'dovich (SZ) clusters discovered in the 268 deg(2) equatorial region survey of the Atacama Cosmology Telescope that overlaps with Sloan Digital Sky Survey (SDSS) Stripe 82 field. Ours is the first weak lensing study with Subaru at such high redshifts. For the weak lensing analysis using i'-band images, we use a model-fitting (Gauss-Laguerre shapelet) method to measure shapes of galaxy images, where we fit galaxy images in different exposures simultaneously to obtain best-fitting ellipticities taking into account the different point spread functions (PSFs) in each exposure. We also take into account the astrometric distortion effect on galaxy images by performing the model fitting in the world coordinate system. To select background galaxies behind the cluster at z = 0.81, we use photometric redshift estimates for every galaxy derived from the co-added images of multi-passband Br'i'z'Y, with PSF matching/homogenization. After a photometric redshift cut for background galaxy selection, we detect the tangential weak lensing distortion signal with a total signal-to-noise ratio of about 3.7. By fitting a Navarro-Frenk-White model to the measured shear profile, we find the cluster mass to be M-200 (rho) over barm = [7.5(-2.8)(+3.2)(stat.)(+1.3)(-0.6)(sys.)] x 10(14) M-circle dot h(-1). The weak lensing-derived mass is consistent with previous mass estimates based on the SZ observation, with assumptions of hydrostatic equilibrium and virial theorem, as well as with scaling relations between SZ signal and mass derived from weak lensing, X-ray and velocity dispersion, within the measurement errors. We also show that the existence of ACT-CL J0022.2-0036 at z = 0.81 is consistent with the cluster abundance prediction of the Lambda-dominated cold dark matter structure formation model. We thus demonstrate the capability of Subaru-type ground-based images for studying weak lensing of high-redshift clusters.
C1 [Miyatake, Hironao; Mineo, Sogo; Aihara, Hiroaki] Univ Tokyo, Dept Phys, Bunkyo Ku, Tokyo 1130031, Japan.
[Miyatake, Hironao; Nishizawa, Atsushi J.; Takada, Masahiro; Mineo, Sogo; Aihara, Hiroaki; Spergel, David N.; Bickerton, Steven J.; Oguri, Masamune; Yasuda, Naoki] Univ Tokyo, WPI, Kavli IPMU, Kashiwa, Chiba 2778582, Japan.
[Miyatake, Hironao; Mandelbaum, Rachel; Spergel, David N.; Bickerton, Steven J.; Lupton, Robert H.; Price, Paul A.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA.
[Mandelbaum, Rachel] Carnegie Mellon Univ, Dept Phys, Pittsburgh, PA 15213 USA.
[Bond, J. Richard; Hajian, Amir; Hincks, Adam D.] Univ Toronto, Canadian Inst Theoret Astrophys, Toronto, ON M5S 3H8, Canada.
[Gralla, Megan; Marriage, Tobias A.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA.
[Hilton, Matt] Univ Nottingham, Sch Phys & Astron, Nottingham NG7 2RD, England.
[Hilton, Matt; Moodley, Kavilan] Univ KwaZulu Natal, Astrophys & Cosmol Res Unit, Sch Math Stat & Comp Sci, ZA-4041 Durban, South Africa.
[Hughes, John P.; Menanteau, Felipe] Rutgers State Univ, Dept Phys & Astron, Piscataway, NJ 08854 USA.
[Infante, Leopoldo; Sifon, Cristobal] Pontificia Univ Catolica Chile, Fac Fis, Dept Astron & Astrofis, Santiago 22, Chile.
[Lin, Yen-Ting] Acad Sinica, Inst Astron & Astrophys, Taipei 115, Taiwan.
[Marsden, Danica] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA.
[Miyazaki, Satoshi] Natl Inst Nat Sci, Natl Astron Observ Japan, Mitaka, Tokyo 1818588, Japan.
[Niemack, Michael D.] NIST, Quantum Devices Grp, Boulder, CO 80305 USA.
[Reese, Erik D.] Univ Penn, Dept Phys & Astron, Philadelphia, PA 19104 USA.
[Sifon, Cristobal] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands.
[Wollack, Edward J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Miyatake, H (reprint author), Univ Tokyo, Dept Phys, Bunkyo Ku, Tokyo 1130031, Japan.
EM miyatake@astro.princeton.edu
RI Wollack, Edward/D-4467-2012; Aihara, Hiroaki/F-3854-2010; Oguri,
Masamune/C-6230-2011; Spergel, David/A-4410-2011; Hilton, Matthew
James/N-5860-2013; Mandelbaum, Rachel/N-8955-2014
OI Wollack, Edward/0000-0002-7567-4451; Menanteau,
Felipe/0000-0002-1372-2534; Sifon, Cristobal/0000-0002-8149-1352;
Aihara, Hiroaki/0000-0002-1907-5964; Mandelbaum,
Rachel/0000-0003-2271-1527
FU MEXT/JSPS [DC1]; JSPS KAKENHI [23340061]; JSPS Core-to-Core Program
'International Research Network for Dark Energy'; World Premier
International Research Center Initiative (WPI Initiative), MEXT, Japan;
FIRST programme 'Subaru Measurements of Images and Redshifts (SuMIRe)',
CSTP, Japan; Alfred P. Sloan Foundation; National Science Foundation; US
Department of Energy Office of Science
FX HM and MT greatly thank Gary Bernstein, Bhuvnesh Jain and Mike Jarvis
for many useful and constructive discussion on the shape measurement
methods. HM acknowledges support by MEXT/JSPS Grant-in-Aid for JSPS
Fellows (DC1). This work is supported in part by JSPS KAKENHI (Grant
Number: 23340061), JSPS Core-to-Core Program 'International Research
Network for Dark Energy', by World Premier International Research Center
Initiative (WPI Initiative), MEXT, Japan, and by the FIRST programme
'Subaru Measurements of Images and Redshifts (SuMIRe)', CSTP, Japan.;
Funding for SDSS-III has been provided by the Alfred P. Sloan
Foundation, the Participating Institutions, the National Science
Foundation and the US Department of Energy Office of Science. The
SDSS-III web site is http://www.sdss3.org/.; SDSS-III is managed by the
Astrophysical Research Consortium for the Participating Institutions of
the SDSS-III Collaboration including the University of Arizona, the
Brazilian Participation Group, Brookhaven National Laboratory,
University of Cambridge, Carnegie Mellon University, University of
Florida, the French Participation Group, the German Participation Group,
Harvard University, the Instituto de Astrofisica de Canarias, the
Michigan State/Notre Dame/JINA Participation Group, The Johns Hopkins
University, Lawrence Berkeley National Laboratory, Max Planck Institute
for Astrophysics, Max Planck Institute for Extraterrestrial Physics, New
Mexico State University, New York University, Ohio State University,
Pennsylvania State University, University of Portsmouth, Princeton
University, the Spanish Participation Group, University of Tokyo,
University of Utah, Vanderbilt University, University of Virginia,
University of Washington and Yale University.
NR 72
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PI OXFORD
PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND
SN 0035-8711
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD MAR
PY 2013
VL 429
IS 4
BP 3627
EP 3644
DI 10.1093/mnras/sts643
PG 18
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 135FD
UT WOS:000318272600072
ER
PT J
AU Dwek, E
Krennrich, F
AF Dwek, Eli
Krennrich, Frank
TI The extragalactic background light and the gamma-ray opacity of the
universe
SO ASTROPARTICLE PHYSICS
LA English
DT Article
DE Extragalactic background light; Cosmic infrared background; Cosmology;
Dark matter; Galaxy evolution; Gamma-ray astronomy; GeV/TeV sources;
Blazars; Gamma-ray opacity
ID SPITZER-SPACE-TELESCOPE; SPECTRAL ENERGY-DISTRIBUTIONS; STAR-FORMATION
HISTORY; LARGE-AREA TELESCOPE; PEAKED BL-LACERTAE; RADIATIVE-TRANSFER
CALCULATIONS; INFRARED LUMINOSITY FUNCTIONS; MICRON SOURCE COUNTS; HARD
TEV SPECTRA; BLAZAR 3C 66A
AB The extragalactic background light (EBL) is one of the fundamental observational quantities in cosmology. All energy releases from resolved and unresolved extragalactic sources, and the light from any truly diffuse background, excluding the cosmic microwave background (CMB), contribute to its intensity and spectral energy distribution. It therefore plays a crucial role in cosmological tests for the formation and evolution of stellar objects and galaxies, and for setting limits on exotic energy releases in the universe. The EBL also plays an important role in the propagation of very high energy gamma-rays which are attenuated en route to Earth by pair producing gamma-gamma interactions with the EBL and CMB. The EBL affects the spectrum of the sources, predominantly blazars, in the similar to 10 GeV-10 TeV energy regime. Knowledge of the EEL intensity and spectrum will allow the determination of the intrinsic blazar spectrum in a crucial energy regime that can be used to test particle acceleration mechanisms and very high energy (VHE) gamma-ray production models. Conversely, knowledge of the intrinsic gamma-ray spectrum and the detection of blazars at increasingly higher redshifts will set strong limits on the EBL and its evolution. This paper reviews the lafest developments in the determination of the EBL and its impact on the current understanding of the origin and production mechanisms of gamma-rays in blazars, and on energy releases in the universe. The review concludes with a summary and future directions in Cherenkov Telescope Array techniques and in infrared ground-based and space observatories that will greatly improve our knowledge of the EBL and the origin and production of very high energy gamma-rays. Published by Elsevier B.V.
C1 [Dwek, Eli] NASA, Observat Cosmol Lab, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Krennrich, Frank] Iowa State Univ, Dept Phys & Astron, Ames, IA 50011 USA.
RP Dwek, E (reprint author), NASA, Observat Cosmol Lab, Goddard Space Flight Ctr, Code 665, Greenbelt, MD 20771 USA.
EM eli.dwek@nasa.gov; krennrich@iastate.edu
FU NASA [NNX11AO38G]; U.S. Department of Energy Office of Science
FX ED and FK gratefully acknowledge the support from the NASA Fermi Guest
Investigator grant NNX11AO38G. FK also acknowledges the support from the
U.S. Department of Energy Office of Science. We thanks C.D. Dermer, J.D.
Finke, A. Dominguez, R.C. Gilmore, A. Franceschini, and J.R. Primack for
providing their model results in digital format. We thank D. Kazanas and
R.G. Arendt for their comments on parts of the manuscript, and an
anonymous referee for his/her thorough reading of and helpful comments
on the manuscript.
NR 244
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U1 0
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PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0927-6505
EI 1873-2852
J9 ASTROPART PHYS
JI Astropart Phys.
PD MAR
PY 2013
VL 43
SI SI
BP 112
EP 133
DI 10.1016/j.astropartphys.2012.09.003
PG 22
WC Astronomy & Astrophysics; Physics, Particles & Fields
SC Astronomy & Astrophysics; Physics
GA 133GL
UT WOS:000318126800010
ER
PT J
AU Moisan, TAH
Moisan, JR
Linkswiler, MA
Steinhardt, RA
AF Moisan, Tiffany A. H.
Moisan, John R.
Linkswiler, Matthew A.
Steinhardt, Rachel A.
TI Algorithm development for predicting biodiversity based on phytoplankton
absorption
SO CONTINENTAL SHELF RESEARCH
LA English
DT Article
DE Phytoplankton; Oceanography; Algorithm; Phytoplankton functional type;
Gulf of Maine; Mid Atlantic Bight
ID SATELLITE OCEAN COLOR; PHAEOCYSTIS-ANTARCTICA KARSTEN; INHERENT
OPTICAL-PROPERTIES; SPECTRAL LIGHT-ABSORPTION; MARINE-PHYTOPLANKTON;
HETEROCAPSA-PYGMAEA; NORTHEAST ATLANTIC; CLASS ABUNDANCES; AMINO-ACIDS;
COMMUNITIES
AB Ocean color remote sensing has provided the scientific community with unprecedented global coverage of chlorophyll a, an indicator of phytoplankton biomass. Together, satellite-derived chlorophyll a and knowledge of Phytoplankton Functional Types (PFTs) will improve our limited understanding of marine ecosystem responses to physiochemical climate drivers involved in carbon cycle dynamics and linkages. Using cruise data from the Gulf of Maine and the Middle Atlantic Bight (N = 269 pairs of HPLC and phytoplankton absorption samples), two modeling approaches were utilized to predict phytoplankton absorption and pigments. Algorithm I predicts the chlorophyll-specific absorption coefficient (a*(ph) (m(2) mg chl a(-1))) using inputs of temperature, light, and chlorophyll a. Modeled r(2) values (400-700 nm) ranged from 0.79 to 0.99 when compared to in situ observations with similar to 25% lower r(2) values in the UV region. Algorithm II-a utilizes matrix inversion analysis to predict a(ph)(m(-1), 400-700 nm) and r(2) values ranged from 0.89 to 0.99. The prediction of phytoplankton pigments with Algorithm II-b produced r(2) values that ranged from 0.40 to 0.93. When used in combination, Algorithm I, and Algorithm II-a are able to use satellite products of SST, PAR, and chlorophyll a (Algorithm I) to predict pigment concentrations and ratios to describe the phytoplankton community. The results of this study demonstrate that the spatial variation in modeled pigment ratios differ significantly from the 10-year SeaWiFS average chlorophyll a data set. Contiguous observations of chlorophyll a and phytoplankton biodiversity will elucidate ecosystem responses with unprecedented complexity. Published by Elsevier Ltd.
C1 [Moisan, Tiffany A. H.; Moisan, John R.] NASA, Goddard Space Flight Ctr, Wallops Flight Facil, Wallops Isl, VA 23337 USA.
[Linkswiler, Matthew A.] NASA, Goddard Space Flight Ctr, Wallops Flight Facil, URS Corp, Wallops Isl, VA 23337 USA.
[Steinhardt, Rachel A.] NASA, Goddard Space Flight Ctr, Wallops Flight Facil, Sigma Space Corp, Wallops Isl, VA 23337 USA.
RP Moisan, TAH (reprint author), NASA, Goddard Space Flight Ctr, Wallops Flight Facil, Wallops Isl, VA 23337 USA.
EM tiffany.a.moisan@nasa.gov
RI Moisan, John/B-8762-2016
OI Moisan, John/0000-0002-8078-8939
FU NASA Biodiversity Program [05-TEB/05-0016]; NOAA; NOAA, U.S. Department
of Commerce [NA03NOS4730220]
FX We thank Ms. Kristin Golmon for earlier testing and development of our
inversion Algorithm through the NASA USRP Student Program. We thank
Carla Makinen and Kristen Blattner for processing absorption data and
participation in filtration and cruise logistics. John Morrow helped to
deploy the PRR-800 on several of the BIOME cruises. We thank Stanley
Hooker (NASA/GSFC) for use of his PAR observations obtained during
several of the cruises in the Gulf of Maine. We thank Antonio Mannino
(NASA/GSFC) for collection of some of the HPLC samples used in the
study. We thank Laurie van Heukelum (HPEL) for processing of the HPLC
samples used in the study (BIOME, COBY, and MAA cruises). We thank
Rachel Steinhardt for her constructive comments and criticisms. We thank
Ms. Olivia Massey for her detailed work on the references. We thank our
reviewers for their excellent and generous comments on our work. Our
work was partially funded by the NASA Biodiversity Program
05-TEB/05-0016 and NOAA. The paper was prepared under award
#NA03NOS4730220 from NOAA, U.S. Department of Commerce. The statements,
findings, and conclusions are those of the authors and do not
necessarily reflect the views of NOAA or the U.S. Department of
Commerce.
NR 79
TC 5
Z9 5
U1 3
U2 48
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0278-4343
EI 1873-6955
J9 CONT SHELF RES
JI Cont. Shelf Res.
PD MAR 1
PY 2013
VL 55
BP 17
EP 28
DI 10.1016/j.csr.2012.12.011
PG 12
WC Oceanography
SC Oceanography
GA 130TU
UT WOS:000317943800002
ER
PT J
AU Giardino, G
Sirianni, M
Birkmann, SM
Rauscher, BJ
Lindler, D
Boker, T
Ferruit, P
De Marchi, G
Stuhlinger, M
Jensen, P
Strada, P
AF Giardino, Giovanna
Sirianni, Marco
Birkmann, Stephan M.
Rauscher, Bernard J.
Lindler, Don
Boker, Torsten
Ferruit, Pierre
De Marchi, Guido
Stuhlinger, Martin
Jensen, Peter
Strada, Paolo
TI Noise properties and signal-dependent interpixel crosstalk of the
detectors of the Near-Infrared Spectrograph of the James Webb Space
Telescope
SO OPTICAL ENGINEERING
LA English
DT Article
DE James Webb Space Telescope; near-infrared spectrograph; near-infrared
detectors; noise; crosstalk
ID EFFICIENCY; ARRAYS
AB The Near-Infrared Spectrograph (NIRSpec) is one of the four science instruments of the James Webb Space Telescope. Its focal plane consists of two HAWAII-2RG sensors operating in the wavelength range of 0.6 to 5.0 mu m and, as part of characterizing NIRSpec, the noise properties of these detectors under dark and illuminated conditions were studied. Under dark conditions, and as already known, 1/f noise in the detector system causes somewhat higher noise levels than can be accounted for by a simple model that includes white read noise and shot noise on integrated charge. More surprisingly, for high levels of accumulated charge, significantly lower total noise than expected was observed. This effect is shown to be due to pixel-to-pixel correlations introduced by signal-dependent interpixel crosstalk, with an interpixel coupling factor, a, that ranges from similar to 0.01 for zero signal to similar to 0.03 close to saturation. (C) 2013 Society of Photo-Optical Instrumentation Engineers (SPIE) [DOI: 10.1117/1.OE.52.3.034001]
C1 [Giardino, Giovanna; Sirianni, Marco; Birkmann, Stephan M.; Boker, Torsten; Ferruit, Pierre; De Marchi, Guido; Jensen, Peter; Strada, Paolo] European Space Agcy, European Space Res & Technol Ctr, NL-2200 AG Noordwijk, Netherlands.
[Rauscher, Bernard J.; Lindler, Don] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Stuhlinger, Martin] European Space Agcy, European Space Astron Ctr, Villanueva De La Cannada, Spain.
RP Giardino, G (reprint author), European Space Agcy, European Space Res & Technol Ctr, Keplerlaan 1, NL-2200 AG Noordwijk, Netherlands.
EM Giovanna.Giardino@esa.int
NR 25
TC 3
Z9 3
U1 0
U2 3
PU SPIE-SOC PHOTO-OPTICAL INSTRUMENTATION ENGINEERS
PI BELLINGHAM
PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98225 USA
SN 0091-3286
EI 1560-2303
J9 OPT ENG
JI Opt. Eng.
PD MAR
PY 2013
VL 52
IS 3
AR 034001
DI 10.1117/1.OE.52.3.034001
PG 8
WC Optics
SC Optics
GA 134XB
UT WOS:000318248000016
ER
PT J
AU Mitchard, ETA
Meir, P
Ryan, CM
Woollen, ES
Williams, M
Goodman, LE
Mucavele, JA
Watts, P
Woodhouse, IH
Saatchi, SS
AF Mitchard, Edward T. A.
Meir, Patrick
Ryan, Casey M.
Woollen, Emily S.
Williams, Mathew
Goodman, Lucy E.
Mucavele, Joey A.
Watts, Paul
Woodhouse, Iain H.
Saatchi, Sassan S.
TI A novel application of satellite radar data: measuring carbon
sequestration and detecting degradation in a community forestry project
in Mozambique
SO PLANT ECOLOGY & DIVERSITY
LA English
DT Article
DE Africa; above-ground biomass; community forestry; forest monitoring;
Miombo; Radar; REDD; REDD; remote sensing; SAR; savanna; woodland
ID WOODY ENCROACHMENT; SAVANNA BOUNDARY; CENTRAL-AFRICA; BIOMASS; COVER;
BACKSCATTER; WOODLANDS; REGION; AMAZON; STOCKS
AB Background: It is essential that systems for measuring changes in carbon stocks for Reducing Emissions from Deforestation and Forest Degradation (REDD) projects are accurate, reliable and low cost. Widely used systems involving classifying optical satellite data can underestimate degradation, and by classifying the landscape ignore the natural heterogeneity of biomass.
Aims: To assess the ability of repeat L-band radar to detect areas of small increases or decreases in above-ground biomass (AGB) across a Miombo woodland landscape.
Methods: ALOS PALSAR L-band cross-polarised (HV) radar data from 2007 and 2009 were used to create maps of AGB, calibrated using 58 field plots. The change in AGB was assessed for land parcels with known landcover histories: (i) 500 ha of new agroforestry; (ii) 9500 ha of protected (REDD) areas; and (iii) 23 ha of land where degradation occurred between 2007 and 2009.
Results: Increases in AGB were detected in both the agroforestry and REDD areas (0.4 and 1.1 Mg C ha(1) year(1), respectively), while the degraded areas showed a decrease of 3 Mg C ha(1) year(1).
Conclusions: PALSAR data can be used to detect losses and gains in AGB in woodland ecosystems. However, further work is needed to precisely quantify the uncertainties in the change estimates, and the extent of false-positive and false-negative change detections that would result from using such a system.
C1 [Mitchard, Edward T. A.; Meir, Patrick; Ryan, Casey M.; Woollen, Emily S.; Williams, Mathew; Woodhouse, Iain H.] Univ Edinburgh, Sch Geosci, Edinburgh, Midlothian, Scotland.
[Goodman, Lucy E.; Mucavele, Joey A.; Watts, Paul] Envirotrade, London, England.
[Saatchi, Sassan S.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
RP Mitchard, ETA (reprint author), Univ Edinburgh, Sch Geosci, Edinburgh, Midlothian, Scotland.
EM edward.mitchard@ed.ac.uk
RI Meir, Patrick/J-8344-2012; Williams, Mathew/G-6140-2016;
OI Williams, Mathew/0000-0001-6117-5208; Mitchard,
Edward/0000-0002-5690-4055; Ryan, Casey/0000-0002-1802-0128
FU European Development Fund; NERC; Envirotrade; Gatsby Plants
FX The European Space Agency provided the ALOS PALSAR scenes for this study
through a Category 1 application to Edward Mitchard. Landsat data were
provided free of charge by the USGS and NASA. The radar data were
originally collected and processed by JAXA. SRTM data were collected by
NASA, and processed by the CGIAR Consortium for Spatial Information
(http://srtm.csi.cgiar.org/). Mapready software, used for processing the
radar data, was provided free of charge by the Alaska Satellite
Facility. The European Development Fund, NERC and Envirotrade funded the
field data collection; Envirotrade also provided logistical support.
Edward Mitchard was funded by Gatsby Plants. We acknowledge the
following Envirotrade employees who assisted in collecting the field
data: Joao 'Dois' Eduardo, Manuel Francisco, Gary Goss, Alfonso Jornal,
Zito Lindo, Neto Moulinho, Salomao 'Baba' Nhangue, Ramaio Saimone with
the supervision of Alastair MacCrimmon, Antonio Serra, and Philip
Powell. Meg Coates-Palgrave carried out the tree identification on the
Permanent Sample Plots. Prof. John Grace, of the University of
Edinburgh, provided invaluable support and advice.
NR 27
TC 13
Z9 15
U1 3
U2 52
PU TAYLOR & FRANCIS LTD
PI ABINGDON
PA 2-4 PARK SQUARE, MILTON PARK, ABINGDON OR14 4RN, OXON, ENGLAND
SN 1755-0874
EI 1755-1668
J9 PLANT ECOL DIVERS
JI Plant Ecol. Divers.
PD MAR 1
PY 2013
VL 6
IS 1
SI SI
BP 159
EP 170
DI 10.1080/17550874.2012.695814
PG 12
WC Plant Sciences
SC Plant Sciences
GA 127ZZ
UT WOS:000317739000012
ER
PT J
AU Puma, MJ
Koster, RD
Cook, BI
AF Puma, Michael J.
Koster, Randal D.
Cook, Benjamin I.
TI Phenological versus meteorological controls on land-atmosphere water and
carbon fluxes
SO JOURNAL OF GEOPHYSICAL RESEARCH-BIOGEOSCIENCES
LA English
DT Article
ID GLOBAL VEGETATION MODEL; LEAF-AREA INDEX; GROSS PRIMARY PRODUCTION;
SURFACE-ENERGY BALANCE; SUB-ALPINE FOREST; CLIMATE MODELS; GISS MODELE;
ECOSYSTEM RESPIRATION; REGIONAL CLIMATE; HIGH-ELEVATION
AB Phenological dynamics and their related processes strongly constrain land-atmosphere interactions, but their relative importance vis-a-vis meteorological forcing within general circulation models (GCMs) is still uncertain. Using an off-line land surface model, we evaluate leaf area and meteorological controls on gross primary productivity, evapotranspiration, transpiration, and runoff at four North American sites, representing different vegetation types and background climates. Our results demonstrate that compared to meteorological controls, variation in leaf area has a dominant control on gross primary productivity, a comparable but smaller influence on transpiration, a weak influence on total evapotranspiration, and a negligible impact on runoff. Climate regime and characteristic variations in leaf area have important modulating effects on these relative controls, which vary depending on the fluxes and timescales of interest. We find that leaf area in energy-limited evaporative regimes tends to exhibit greater control on annual gross primary productivity than in moisture-limited regimes, except when vegetation exhibits little interannual variation in leaf area. For transpiration, leaf area control is somewhat less in energy-limited regimes and greater in moisture-limited regimes for maximum pentad and annual fluxes. These modulating effects of climate and leaf area were less clear for other fluxes and at other timescales. Our findings are relevant to land-atmosphere coupling in GCMs, especially considering that leaf area variations are a fundamental element of land use and land cover change simulations. Citation: Puma, M. J., R. D. Koster, and B. I. Cook (2013), Phenological versus meteorological controls on land-atmosphere water and carbon fluxes, J. Geophys. Res. Biogeosci., 118, 14-29, doi:10.1029/2012JG002088.
C1 [Puma, Michael J.] Columbia Univ, Ctr Climate Syst Res, New York, NY 10025 USA.
[Puma, Michael J.; Cook, Benjamin I.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
[Koster, Randal D.] NASA, Global Modeling & Assimilat Off, Goddard Space Flight Ctr, Greenbelt, MD USA.
RP Puma, MJ (reprint author), Columbia Univ, Ctr Climate Syst Res, 2880 Broadway, New York, NY 10025 USA.
EM mjp38@columbia.edu
RI Cook, Benjamin/H-2265-2012; Koster, Randal/F-5881-2012;
OI Koster, Randal/0000-0001-6418-6383; Puma, Michael/0000-0002-4255-8454
FU NASA [NNX08AJ75A]; NASA Climate and Earth Observing Program; AmeriFlux
sites by the Department of Energy's Climate and Environmental Sciences
Division within the Office of Biological and Environmental Research
FX The authors gratefully acknowledge funding for Interdisciplinary Global
Change Research under NASA cooperative agreement NNX08AJ75A supported by
the NASA Climate and Earth Observing Program. The Collection 4 MODIS LAI
(MOD15A2) data were obtained through the online Data Pool at the NASA
Land Processes Distributed Active Archive Center (LP DAAC,
http://lpdaac.usgs.gov/get_data). Meteorological driver and validation
data were collected and prepared by the individual AmeriFlux site
principal investigators and their teams, so we would like to extend our
thanks to J. William Munger (Harvard Forest), Tilden Meyers (Bondville),
and Peter Blanken and Russell Monson (Niwot Ridge). We also recognize
funding of AmeriFlux sites by the Department of Energy's Climate and
Environmental Sciences Division within the Office of Biological and
Environmental Research. Finally, we would like to thank the anonymous
reviewers, whose comments greatly improved this paper.
NR 82
TC 10
Z9 10
U1 3
U2 43
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-8953
EI 2169-8961
J9 J GEOPHYS RES-BIOGEO
JI J. Geophys. Res.-Biogeosci.
PD MAR
PY 2013
VL 118
IS 1
BP 14
EP 29
DI 10.1029/2012JG002088
PG 16
WC Environmental Sciences; Geosciences, Multidisciplinary
SC Environmental Sciences & Ecology; Geology
GA 129MN
UT WOS:000317844700002
ER
PT J
AU Kasischke, ES
Amiro, BD
Barger, NN
French, NHF
Goetz, SJ
Grosse, G
Harmon, ME
Hicke, JA
Liu, SG
Masek, JG
AF Kasischke, Eric S.
Amiro, Brian D.
Barger, Nichole N.
French, Nancy H. F.
Goetz, Scott J.
Grosse, Guido
Harmon, Mark E.
Hicke, Jeffrey A.
Liu, Shuguang
Masek, Jeffrey G.
TI Impacts of disturbance on the terrestrial carbon budget of North America
SO JOURNAL OF GEOPHYSICAL RESEARCH-BIOGEOSCIENCES
LA English
DT Article
ID MOUNTAIN PINE-BEETLE; FOREST GAP MODELS; ICE STORM DAMAGE;
CLIMATE-CHANGE; UNITED-STATES; PERMAFROST THAW; FIRE SEVERITY; BOREAL
FOREST; DYNAMICS; CANADA
AB Because it is an important regulator of terrestrial carbon cycling in North America, extensive research on natural and human disturbances has been carried out as part of the North American Carbon Program and the CarboNA project. A synthesis of various components of this research was carried out, and the results are presented in the papers contained in this special section. While the synthesis primarily focused on the impacts of fire, insects/disease, and harvesting on terrestrial carbon cycling in forests, several groups focused on impacts of disturbance on woody encroachment in western U. S. dry lands and on soil carbon present in northern high-latitude regions. Here, we present a summary of the results from these papers, along with the findings and recommendations from the disturbance synthesis. Citation: Kasischke, E. S., B. D. Amiro, N. N. Barger, N. H. F. French, S. J. Goetz, G. Grosse, M. E. Harmon, J. A. Hicke, S. Liu, and J. G. Masek (2013), Impacts of disturbance on the terrestrial carbon budget of North America, J. Geophys. Res. Biogeosci., 118, 303-316, doi:10.1002/jgrg.20027.
C1 [Kasischke, Eric S.] Univ Maryland, Dept Geog Sci, College Pk, MD 20742 USA.
[Amiro, Brian D.] Univ Manitoba, Dept Soil Sci, Winnipeg, MB, Canada.
[Barger, Nichole N.] Univ Colorado, Dept Ecol & Evolutionary Biol, Boulder, CO 80309 USA.
[French, Nancy H. F.] Michigan Technol Univ, Michigan Tech Res Inst, Ann Arbor, MI USA.
[Goetz, Scott J.] Woods Hole Res Ctr, Falmouth, MA USA.
[Grosse, Guido] Univ Alaska Fairbanks, Inst Geophys, Fairbanks, AK 99775 USA.
[Harmon, Mark E.] Oregon State Univ, Dept Forest Ecosyst & Soc, Corvallis, OR 97331 USA.
[Hicke, Jeffrey A.] Univ Idaho, Dept Geog, Moscow, ID 83843 USA.
[Liu, Shuguang] US Geol Survey, Earth Resources Observat & Sci Ctr, Sioux Falls, SD USA.
[Masek, Jeffrey G.] NASA, Goddard Space Flight Ctr, Biospher Sci Branch, Greenbelt, MD 20771 USA.
RP Kasischke, ES (reprint author), Univ Maryland, Dept Geog Sci, 2181 LeFrak Hall, College Pk, MD 20742 USA.
EM ekasisch@umd.edu
RI Grosse, Guido/F-5018-2011; Masek, Jeffrey/D-7673-2012; Hicke,
Jeff/M-9677-2013; Goetz, Scott/A-3393-2015;
OI Grosse, Guido/0000-0001-5895-2141; Goetz, Scott/0000-0002-6326-4308;
French, Nancy/0000-0002-2389-3003
FU NASA [NNX08AK69G, NNX09AP53G, NNX08AG13G, NNX08AJ37, NNX08AI79G]; NOAA
[NA08OAR4310526]; NSF [0902056, OPP-0732735]; USGS Western Mountain
Initiative, U.S.F.S. Western Wildland Environmental Threat Assessment
Center, National Institute for Climate Change Research (Department of
Energy); University of Idaho NSF EPSCoR
FX The authors thank the U.S. Geological Survey for providing travel
support for attendees of a disturbance synthesis workshop, held in
Reston, Virginia, 28-30 October 2009. N.H.F.F. was supported by NASA
Carbon Cycle Science Program grant NNX08AK69G and NASA Applied Science
Program grant NNX09AP53G. S.J.G. acknowledges support from NOAA Global
Carbon Cycle Program grant NA08OAR4310526, NASA Carbon Cycle and
Ecosystems Program grant NNX08AG13G, and NSF Seasonality grant 0902056.
G. G. was supported by NSF grant OPP-0732735 and NASA grant NNX08AJ37.
J.A.H. was supported by the USGS Western Mountain Initiative, U.S.F.S.
Western Wildland Environmental Threat Assessment Center, National
Institute for Climate Change Research (Department of Energy), and the
University of Idaho NSF EPSCoR grant. E. S. K. was supported by NASA
Carbon Cycle Science Program grant NNX08AI79G. J.G.M. was supported by
NASA's Terrestrial Ecology Program.
NR 89
TC 22
Z9 22
U1 2
U2 139
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-8953
EI 2169-8961
J9 J GEOPHYS RES-BIOGEO
JI J. Geophys. Res.-Biogeosci.
PD MAR
PY 2013
VL 118
IS 1
BP 303
EP 316
DI 10.1002/jgrg.20027
PG 14
WC Environmental Sciences; Geosciences, Multidisciplinary
SC Environmental Sciences & Ecology; Geology
GA 129MN
UT WOS:000317844700025
ER
PT J
AU Hayne, PO
AF Hayne, Paul O.
TI Abandoned frontier
SO NATURE GEOSCIENCE
LA English
DT Editorial Material
C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Hayne, PO (reprint author), CALTECH, Jet Prop Lab, MS 183-301, Pasadena, CA 91109 USA.
EM Paul.O.Hayne@jpl.nasa.gov
NR 2
TC 2
Z9 2
U1 0
U2 2
PU NATURE PUBLISHING GROUP
PI NEW YORK
PA 75 VARICK ST, 9TH FLR, NEW YORK, NY 10013-1917 USA
SN 1752-0894
J9 NAT GEOSCI
JI Nat. Geosci.
PD MAR
PY 2013
VL 6
IS 3
BP 155
EP 156
DI 10.1038/ngeo1753
PG 2
WC Geosciences, Multidisciplinary
SC Geology
GA 117IC
UT WOS:000316945800003
ER
PT J
AU Randel, WJ
Jensen, EJ
AF Randel, William J.
Jensen, Eric J.
TI Physical processes in the tropical tropopause layer and their roles in a
changing climate
SO NATURE GEOSCIENCE
LA English
DT Review
ID BREWER-DOBSON CIRCULATION; LOWER-STRATOSPHERIC TEMPERATURES; ASIAN
MONSOON TRANSPORT; ANNUAL CYCLE; WATER-VAPOR; UPPER TROPOSPHERE; CIRRUS
FORMATION; DEEP CONVECTION; ICE NUCLEATION; CLOUD
AB Tropical climate and the composition of the global upper atmosphere are affected by the tropical tropopause layer - the atmospheric transition zone between the well-mixed, convective troposphere (up to altitudes of 12-14 km) and the highly stratified stratosphere (above about 18 km). Featuring chemical and dynamical properties that are midway between those of the troposphere and stratosphere, the tropopause layer is maintained by a complex interplay between large-and small-scale circulation patterns, deep convection, clouds and radiation. Tropospheric air enters the stratosphere primarily in the tropics. Ozone-and aerosol-related constituents of the global stratosphere, as well as water vapour content, are therefore largely determined by the composition of the air near the tropical tropopause. Over the past years, it has emerged that both slow ascent and rapid deep convection contribute to the composition and thermal structure of the tropical tropopause layer. Ice formation processes at low temperatures affect the efficacy of freeze drying as air passes through the cold tropopause region. Transport and mixing in the tropopause region has been found to be closely linked with the Asian monsoon and other tropical circulation systems. Given these connections, climate change is expected to influence the tropopause layer, for example through enhanced large-scale upwelling of air and potential changes in tropical convection, air temperature, chemical composition and cirrus.
C1 [Randel, William J.] Natl Ctr Atmospher Res, Boulder, CO 80307 USA.
[Jensen, Eric J.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
RP Randel, WJ (reprint author), Natl Ctr Atmospher Res, POB 3000, Boulder, CO 80307 USA.
EM randel@ucar.edu
RI Randel, William/K-3267-2016
OI Randel, William/0000-0002-5999-7162
NR 93
TC 77
Z9 78
U1 6
U2 85
PU NATURE PUBLISHING GROUP
PI NEW YORK
PA 75 VARICK ST, 9TH FLR, NEW YORK, NY 10013-1917 USA
SN 1752-0894
EI 1752-0908
J9 NAT GEOSCI
JI Nat. Geosci.
PD MAR
PY 2013
VL 6
IS 3
BP 169
EP 176
DI 10.1038/ngeo1733
PG 8
WC Geosciences, Multidisciplinary
SC Geology
GA 117IC
UT WOS:000316945800014
ER
PT J
AU Hui, HJ
Peslier, AH
Zhang, YX
Neal, CR
AF Hui, Hejiu
Peslier, Anne H.
Zhang, Youxue
Neal, Clive R.
TI Water in lunar anorthosites and evidence for a wet early Moon
SO NATURE GEOSCIENCE
LA English
DT Article
ID MAGMA OCEAN; ORIGIN; MANTLE; HYDROGEN; SURFACE; IMPACT; SPECIATION;
FELDSPARS; PETROLOGY; HYDROXYL
AB The Moon was thought to be anhydrous since the Apollo era(1), but this view has been challenged by detections of water on the lunar surface(2-4) and in volcanic rocks(5-9) and regolith(10). Part of this water is thought to have been brought through solar-wind implantation(2-4,7,10) and meteorite impacts(2,3,7,11), long after the primary lunar crust formed from the cooling magma ocean(12,13). Here we show that this primary crust of the Moon contains significant amounts of water. We analysed plagioclase grains in lunar anorthosites thought to sample the primary crust, obtained in the Apollo missions, using Fourier-transform infrared spectroscopy, and detected approximately 6 ppm water. We also detected up to 2.7 ppm water in plagioclase grains in troctolites also from the lunar highland upper crust. From these measurements, we estimate that the initial water content of the lunar magma ocean was approximately 320 ppm; water accumulating in the final residuum of the lunar magma ocean could have reached 1.4 wt%, an amount sufficient to explain water contents measured in lunar volcanic rocks. The presence of water in the primary crust implies a more prolonged crystallization of the lunar magma ocean than a dry moon scenario and suggests that water may have played a key role in the genesis of lunar basalts.
C1 [Hui, Hejiu; Neal, Clive R.] Univ Notre Dame, Dept Civil & Environm Engn & Earth Sci, Notre Dame, IN 46556 USA.
[Peslier, Anne H.] Jacobs Technol, ESCG, Houston, TX 77058 USA.
[Peslier, Anne H.] NASA, ARES, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA.
[Zhang, Youxue] Univ Michigan, Dept Earth & Environm Sci, Ann Arbor, MI 48109 USA.
RP Hui, HJ (reprint author), Univ Notre Dame, Dept Civil & Environm Engn & Earth Sci, Notre Dame, IN 46556 USA.
EM hhui@nd.edu
RI Hui, Hejiu/D-2912-2011
OI Hui, Hejiu/0000-0003-2733-5794
FU NASA [NNX11AH48G, NNX10AH74G]
FX This work was supported by NASA (NNX11AH48G to H.H. and NNX10AH74G to
Y.Z.). We thank the Apollo sample curators for allocating us the samples
and G. Rossman for providing an aliquot of plagioclase GRR1968. H.H.
thanks Y. Chen for technical assistance on heating experiments and
electron microprobe analyses, and D. Draper and the LPI for help to
access the JSC facility. This manuscript was greatly improved by the
suggestions and comments of E. A. Johnson.
NR 30
TC 63
Z9 66
U1 2
U2 56
PU NATURE PUBLISHING GROUP
PI NEW YORK
PA 75 VARICK ST, 9TH FLR, NEW YORK, NY 10013-1917 USA
SN 1752-0894
J9 NAT GEOSCI
JI Nat. Geosci.
PD MAR
PY 2013
VL 6
IS 3
BP 177
EP 180
DI 10.1038/ngeo1735
PG 4
WC Geosciences, Multidisciplinary
SC Geology
GA 117IC
UT WOS:000316945800015
ER
PT J
AU Coustenis, A
Atreya, S
Castillo, J
Coll, P
Mueller-Wodarg, I
Spilker, L
AF Coustenis, A.
Atreya, S.
Castillo, J.
Coll, P.
Mueller-Wodarg, I.
Spilker, L.
TI Surfaces, atmospheres and magnetospheres of the outer planets and their
satellites and ring systems: Part VIII Preface
SO PLANETARY AND SPACE SCIENCE
LA English
DT Editorial Material
C1 [Coustenis, A.] Observ Paris, LESIA, F-92195 Meudon, France.
[Atreya, S.] Univ Michigan, Ann Arbor, MI 48109 USA.
[Castillo, J.] JPL Caltech, Pasadena, CA USA.
[Coll, P.] Univ Paris 07, LISA, Creteil, France.
[Coll, P.] Hop Henri Mondor, CNRS, F-94010 Creteil, France.
[Mueller-Wodarg, I.] Univ London Imperial Coll Sci Technol & Med, London, England.
[Spilker, L.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
RP Coustenis, A (reprint author), Observ Paris, LESIA, F-92195 Meudon, France.
EM athena.coustenis@obspm.fr
RI Mueller-Wodarg, Ingo/M-9945-2014
OI Mueller-Wodarg, Ingo/0000-0001-6308-7826
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PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0032-0633
J9 PLANET SPACE SCI
JI Planet Space Sci.
PD MAR
PY 2013
VL 77
SI SI
BP 1
EP 2
DI 10.1016/j.pss.2013.01.002
PG 2
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 127PS
UT WOS:000317711500001
ER
PT J
AU Panchenko, M
Rucker, HO
Farrell, WM
AF Panchenko, M.
Rucker, H. O.
Farrell, W. M.
TI Periodic bursts of Jovian non-Io decametric radio emission
SO PLANETARY AND SPACE SCIENCE
LA English
DT Article
DE Jovian radio emission; Jovian decametric radio emission; Periodic radio
bursts; Jovian radio arcs; Jupiter-Io interaction; DAM
ID PLASMA TORUS; SOLAR-WIND; NUMERICAL-SIMULATION; JUPITER; ULYSSES;
MAGNETOSPHERE; VARIABILITY; ENCOUNTER; TRANSPORT; DRIVEN
AB During the years 2000-2011 the radio instruments onboard Cassini, Wind and STEREO spacecraft have recorded a large amount of the Jovian decametric radio emission (DAM). In this paper we report on the analysis of the new type of Jovian periodic radio bursts recently revealed in the decametric frequency range. These bursts, which are non-In component of DAM, are characterized by a strong periodic reoccurrence over several Jovian days with a period approximate to 1.5% longer than the rotation rate of the planet's magnetosphere (System III). The bursts are typically observed between 4 and 12 MHz and their occurrence probability has been found to be significantly higher in the sector of Jovian Central Meridian Longitude between 300 degrees and 60 degrees (via 360 degrees). The stereoscopic multispacecraft observations have shown that the radio sources of the periodic bursts radiate in a non-axisymmetric hollow cone-like pattern and sub-corotate with Jupiter remaining active during several planet's rotations. The occurrence of the periodic non-Io DAM bursts is strongly correlated with pulses of the solar wind ram pressure at Jupiter. Moreover the periodic bursts exhibit a tendency to occur in groups every similar to 25 days. The polarization measurements have shown that the periodic bursts are right hand polarized radio emission associated with the Northern magnetic hemisphere of Jupiter. We suggest that periodic non-Io DAM bursts may be connected with the interchange instability in Io plasma torus triggered by the solar wind. (C) 2012 Elsevier Ltd. All rights reserved.
C1 [Panchenko, M.; Rucker, H. O.] Space Res Inst AAS, Graz, Austria.
[Farrell, W. M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Panchenko, M (reprint author), Space Res Inst AAS, Graz, Austria.
EM mykhaylo.panchenko@oeaw.ac.at
RI Farrell, William/I-4865-2013
FU Austrian Science Fund (FWF) [P23762-N16, P20680-N16]
FX The authors are pleased to acknowledge the Plasma Physics Data Center
(CDPP), ESA data Archive, STEREO/WAVES, Wind/WAVES, Cassini/RPWS,
Ulysses/URAP and Ulysses/SWOOPS teams for access to data. This work was
financed by the Austrian Science Fund (FWF projects P23762-N16 and
P20680-N16). The authors are grateful to the referees for their helpful
comments that improved this paper.
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SN 0032-0633
J9 PLANET SPACE SCI
JI Planet Space Sci.
PD MAR
PY 2013
VL 77
SI SI
BP 3
EP 11
DI 10.1016/j.pss.2012.08.015
PG 9
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 127PS
UT WOS:000317711500002
ER
PT J
AU Lipatov, AS
Cooper, JF
Paterson, WR
Sittler, EC
Hartle, RE
Simpson, DG
AF Lipatov, A. S.
Cooper, J. F.
Paterson, W. R.
Sittler, E. C., Jr.
Hartle, R. E.
Simpson, D. G.
TI Jovian plasma torus interaction with Europa. Plasma wake structure and
effect of inductive magnetic field: 3D hybrid kinetic simulation
SO PLANETARY AND SPACE SCIENCE
LA English
DT Article
DE Europa; Jovian magnetosphere; Plasma; Magnetic fields; Ion composition
ID IOS INTERACTION; SOLAR-WIND; MAGNETOSPHERIC INTERACTION; SUBSURFACE
OCEAN; MHD SIMULATION; CURRENT SYSTEM; ENVIRONMENT; ATMOSPHERE; MODEL;
CALLISTO
AB The hybrid kinetic model supports comprehensive simulation of the interaction between different spatial and energetic elements of the Europa moon-magnetosphere system with respect to a variable upstream magnetic field and flux or density distributions of plasma and energetic ions, electrons, and neutral atoms. This capability is critical for improving the interpretation of the existing Europa flyby measurements from the Galileo Orbiter mission, and for planning flyby and orbital measurements (including the surface and atmospheric compositions) for future missions. The simulations are based on recent models of the atmosphere of Europa (Cassidy et al., 2007; Shematovich et al., 2005). In contrast to previous approaches with MHD simulations, the hybrid model allows us to fully take into account the finite gyroradius effect and electron pressure, and to correctly estimate the ion velocity distribution and the fluxes along the magnetic field (assuming an initial Maxwellian velocity distribution for upstream background ions). Photoionization, electron-impact ionization, charge exchange and collisions between the ions and neutrals are also included in our model. We consider the models with O+ + and S+ + background plasma, and various betas for background ions and electrons, and pickup electrons. The majority of O-2 atmosphere is thermal with an extended non-thermal population (Cassidy et al., 2007). In this paper, we discuss two tasks: (1) the plasma wake structure dependence on the parameters of the upstream plasma and Europa's atmosphere (model I, cases (a) and (b) with a homogeneous Jovian magnetosphere field, an inductive magnetic dipole and high oceanic shell conductivity); and (2) estimation of the possible effect of an induced magnetic field arising from oceanic shell conductivity. This effect was estimated based on the difference between the observed and modeled magnetic fields (model II, case (c) with an inhomogeneous Jovian magnetosphere field, an inductive magnetic dipole and low oceanic shell conductivity). (C) 2013 Elsevier Ltd. All rights reserved.
C1 [Lipatov, A. S.] UMBC NASA GSFC, Goddard Planetary Heliophys Inst, Greenbelt, MD 20771 USA.
[Lipatov, A. S.; Cooper, J. F.; Paterson, W. R.; Sittler, E. C., Jr.; Hartle, R. E.; Simpson, D. G.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Lipatov, A. S.] Moscow Inst Phys & Technol, Dept Problems Phys & Power Engn, Moscow, Russia.
RP Lipatov, AS (reprint author), NASA, Goddard Space Flight Ctr, Code 673,Bld 21,Rm 247,8800 Greenbelt Rd, Greenbelt, MD 20771 USA.
EM Alexander.Lipatov-1@nasa.gov; John.F.Cooper@nasa.gov;
William.R.Paterson@nasa.gov; Edward.C.Sittler@nasa.gov;
Richard.E.Hartle@nasa.gov; David.G.Simpson@nasa.gov
RI Cooper, John/D-4709-2012
FU GPHI UMBC [00004129, 00004549]; NASA GSFC [00004129, 00004549]; NASA
Outer Planets Research Program; NASA Ames Advanced Supercomputing
Division (SGI-Columbia) [SMD-09-1110]
FX A.S.L. was supported in part by the Project/Grant 00004129, and 00004549
between the GPHI UMBC and NASA GSFC. J.F.C. was supported as Principal
Investigator by the NASA Outer Planets Research Program. Computational
resources were provided by the NASA Ames Advanced Supercomputing
Division (SGI-Columbia, Project SMD-09-1110).
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SN 0032-0633
J9 PLANET SPACE SCI
JI Planet Space Sci.
PD MAR
PY 2013
VL 77
SI SI
BP 12
EP 24
DI 10.1016/j.pss.2013.01.009
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 127PS
UT WOS:000317711500003
ER
PT J
AU Baines, KH
Yanamandra-Fisher, PA
Momary, TW
Orton, GS
Villar, GG
Fletcher, LN
Campins, H
Rivkin, AS
Shara, M
AF Baines, Kevin H.
Yanamandra-Fisher, Padmavati A.
Momary, Thomas W.
Orton, Glenn S.
Villar, Gregorio G., III
Fletcher, Leigh N.
Campins, Humberto
Rivkin, Andrew S.
Shara, Michael
TI The temporal evolution of the July 2009 Jupiter impact cloud
SO PLANETARY AND SPACE SCIENCE
LA English
DT Article
DE Jupiter: clouds; Planetary atmospheres; Atmospheric impacts
ID PROBE MASS-SPECTROMETER; ENTRY SITE; GALILEO; ATMOSPHERE; NEPTUNE;
METHANE; DEBRIS; ABSORPTION; PARAMETERS; SCATTERING
AB Clouds formed on Jupiter by the impact of July 19, 2009 were observed from the IRTF with the same instrument and near-infrared filters during four observing runs over 50 days, beginning one day after impact, providing comprehensive diagnostics of cloudtop altitude, particle size and opacity and yielding quantitative information on the temporal evolution of the impact cloud (IC). The IC evolved relatively rapidly during the first 26 days after impact (Period I) and relatively slowly for the next 23 days (Period II). For the column volume density of the IC core, analyzed over a range of models with varying Mie-scattering particle radii over 0.1-1.1 mu m and imaginary indices of refraction (n(i)) from 0.001 to the limiting model-constrained value of 0.03, the Period I e-folding timescale is 4-16 times less than for Period II, with a best-fit timescale of of 23 days (Period I) increasing to 117 days (Period II) for the nominal best-fit case of large (0.7-1.1 mu m) dark (n(i)=0.01) particles consistent with previous determinations of the size and near-infrared brightness of impact cloud particles (de Pater et al. Icarus 210, 722-741, 2010). Over the entire period, the nominal model mean particle radius ranges from similar to 0.85 mu m one day after impact to 0.89-1.06 mu m 49 days later, considerably larger than the 0.21-0.28 mu m particles determined for the Shoemaker Levy 9 impact (SL9; West et al., Science 267, 1296-1301, 1995). The 1.69 and 2.12 mu m nominal model IC core opacities show timescales averaged over the entire seven-week period of similar to 33 and similar to 35 days, respectively, similar to 60% longer than the 18-23 day timescales of small-particle models (-0.36 mu m radius) which are more consistent with the similar to 15-day visible timescale reported by Sanchez-Lavega et al. (2011, Icarus 214,462-476). Including the area of the entire IC, we find that the total particle volume over the 49 days changes from similar to 0.036 to similar to 0.022 km(3) for the nominal model, corresponding to a variation of the diameter of an equivalent sphere from similar to 0.41 to similar to 035 km, close to the similar to 10% diameter change over one month reported for SL9 clouds (West et al, ibid). Nominal Period II timescales for opacities and total cloud volume - 50-300 days - are 2-11 times longer than nominal Period I timescales; indeed, values of infinity are consistent with the uncertainties. The relatively long timescales found for total cloud dissipation are consistent with (1) material dispersal by wind shears, and (2) relatively weak sedimentation/coagulation, consistent with SL9 results (West et al., ibid). Finally, the IC thickness of similar to 1 scale-height permits a vertical windshear of similar to 1 m/s, inconsistent with the derived similar to 7 m/s cloud spreading, thus implying that the meridional shear is the dominant cloud shear component, as reported for visible measurements (Sanchez-Lavega et al. ibid). (C) 2012 Elsevier Ltd. All rights reserved.
C1 [Baines, Kevin H.; Momary, Thomas W.; Orton, Glenn S.; Villar, Gregorio G., III] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Yanamandra-Fisher, Padmavati A.] Space Sci Inst, Boulder, CO 80301 USA.
[Fletcher, Leigh N.] Univ Oxford, Oxford OX1 3PU, England.
[Campins, Humberto] Univ Cent Florida, Dept Phys, Orlando, FL 32816 USA.
[Rivkin, Andrew S.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA.
[Shara, Michael] Amer Museum Nat Hist, Dept Astrophys, New York, NY 10024 USA.
RP Baines, KH (reprint author), CALTECH, Jet Prop Lab, M-S 183-601,4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM kevin.baines@jpl.nasa.gov; padma@spacescience.org;
thomas.w.momary@jpl.nasa.gov; go@orton.jpl.nasa.gov;
gregorio.g.villar.III@jpl.nasa.gov; fletcher@atm.ox.ac.uk;
campins@physics.ucf.edi; andy.rivkin@jhuapl.edu; mshara@amnh.org
RI Fletcher, Leigh/D-6093-2011; Rivkin, Andrew/B-7744-2016
OI Fletcher, Leigh/0000-0001-5834-9588; Rivkin, Andrew/0000-0002-9939-9976
FU National Aeronautics and Space Administration; University of Oxford
FX We thank the IRTF Telescope Operator Staff, including William Golisch,
David Griep and and Paul Sears. Much of the work described in this paper
was carried out in part at the Jet Propulsion Laboratory, Pasadena,
California, under contract with the National Aeronautics and Space
Administration. Fletcher was supported as a Glasstone Research Fellow at
the University of Oxford. During a portion of this research, Villar was
a NASA Undergraduate Student Research Program (USRP) fellow. Orton and
Yanamandra-Fisher were visiting astronomers at the Infrared Telescope
Facility, which is operated by the University of Hawaii under
Cooperative Agreement number NCC 5-538 with the National Aeronautics and
Space Administration. We would like to thank two anonymous reviewers for
valuable and helpful comments.
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SN 0032-0633
J9 PLANET SPACE SCI
JI Planet Space Sci.
PD MAR
PY 2013
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DI 10.1016/j.pss.2012.05.007
PG 15
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 127PS
UT WOS:000317711500004
ER
PT J
AU Dalton, JB
Cassidy, T
Paranicas, C
Shirley, JH
Prockter, LM
Kamp, LW
AF Dalton, J. B., III
Cassidy, T.
Paranicas, C.
Shirley, J. H.
Prockter, L. M.
Kamp, L. W.
TI Exogenic controls on sulfuric acid hydrate production at the surface of
Europa
SO PLANETARY AND SPACE SCIENCE
LA English
DT Article
DE Europa; Infrared spectroscopy; Magnetosphere
ID INFRARED MAPPING SPECTROMETER; ICY GALILEAN SATELLITES; WATER-ICE;
ELECTRON-BOMBARDMENT; SUBSURFACE OCEAN; SALT MINERALS; SPECTROSCOPY;
ORIGIN; CHAOS; LIFE
AB External agents have heavily weathered the visible surface of Europa. Internal and external drivers competing to produce the surface we see include, but are not limited to: aqueous alteration of materials within the icy shell, initial emplacement of endogenic material by geologic activity, implantation of exogenic ions and neutrals from Jupiter's magnetosphere, alteration of surface chemistry by radiolysis and photolysis, impact gardening of upper surface layers, and redeposition of sputtered volatiles. Separating the influences of these processes is critical to understanding the surface and subsurface compositions at Europa. Recent investigations have applied cryogenic reflectance spectroscopy to Galileo Near-Infrared Mapping Spectrometer (NIMS) observations to derive abundances of surface materials including water ice, hydrated sulfuric acid, and hydrated sulfate salts. Here we compare derived sulfuric acid hydrate (H2SO4 center dot nH(2)O) abundance with weathering patterns and intensities associated with charged particles from Jupiter's magnetosphere. We present models of electron energy, ion energy, and sulfur ion number flux as well as the total combined electron and ion energy flux at the surface to estimate the influence of these processes on surface concentrations, as a function of location. We found that correlations exist linking both electron energy flux (r similar to 0.75) and sulfur ion flux (r=0.93) with the observed abundance of sulfuric acid hydrate on Europa. Sulfuric acid hydrate production on Europa appears to be limited in some regions by a reduced availability of sulfur ions, and in others by insufficient levels of electron energy. The energy delivered by sulfur and other ions has a much less significant role. Surface deposits in regions of limited exogenic processing are likely to bear closest resemblance to oceanic composition. These results will assist future efforts to separate the relative influence of endogenic and exogenic sources in establishing the surface composition. (C) 2012 Elsevier Ltd. All rights reserved.
C1 [Dalton, J. B., III; Cassidy, T.; Shirley, J. H.; Kamp, L. W.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Paranicas, C.; Prockter, L. M.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA.
RP Dalton, JB (reprint author), CALTECH, Jet Prop Lab, Mail Stop 183-301,4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM dalton@jpl.nasa.gov; Timothy.Cassidy@lasp.colorado.edu;
Chris.Paranicas@jhuapl.edu; James.H.Shirley@jpl.nasa.gov;
Louise.Prockter@jhuapl.edu; lwk@mipl.jpl.nasa.gov
RI Paranicas, Christopher/B-1470-2016
OI Paranicas, Christopher/0000-0002-4391-8255
FU NASA Outer Planets Research Program
FX Comments from an anonymous reviewer led to significant improvements in
this manuscript. We gratefully acknowledge the support of the NASA Outer
Planets Research Program. Parts of this work were carried out at the Jet
Propulsion Laboratory, California Institute of Technology, and at the
Johns Hopkins Applied Physics Laboratory.
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SN 0032-0633
J9 PLANET SPACE SCI
JI Planet Space Sci.
PD MAR
PY 2013
VL 77
SI SI
BP 45
EP 63
DI 10.1016/j.pss.2012.05.013
PG 19
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 127PS
UT WOS:000317711500006
ER
PT J
AU Cassidy, TA
Paranicas, CP
Shirley, JH
Dalton, JB
Teolis, BD
Johnson, RE
Kamp, L
Hendrix, AR
AF Cassidy, T. A.
Paranicas, C. P.
Shirley, J. H.
Dalton, J. B., III
Teolis, B. D.
Johnson, R. E.
Kamp, L.
Hendrix, A. R.
TI Magnetospheric ion sputtering and water ice grain size at Europa
SO PLANETARY AND SPACE SCIENCE
LA English
DT Article
DE Europa; Water Ice Sputtering Yields; Galileo NIMS Data Analysis
ID GALILEAN SATELLITES; ATMOSPHERE; TORUS; CONSTRAINTS; GANYMEDE; MODEL
AB We present the first calculation of Europa's sputtering (ion erosion) rate as a function of position on Europa's surface. We find a global sputtering rate of 2 x 10(27) H2O s(-1), some of which leaves the surface in the form of O-2 and H-2. The calculated O-2 production rate is 1 x 10(26) O-2 s(-1), H-2 production is twice that value. The total sputtering rate (including all species) peaks at the trailing hemisphere apex and decreases to about 1/3rd of the peak value at the leading hemisphere apex. O-2 and H-2 sputtering, by contrast, is confined almost entirely to the trailing hemisphere. Most sputtering is done by energetic sulfur ions (100s of keV to MeV), but most of the O-2 and H-2 production is done by cold oxygen ions (temperature similar to 100 eV, total energy similar to 500 eV). As a part of the sputtering rate calculation we compared experimental sputtering yields with analytic estimates. We found that the experimental data are well approximated by the expressions of Fama et al. for ions with energies less than 100 keV (Fama, M., Shi, J., Baragiola, R.A., 2008. Sputtering of ice by low-energy ions. Surf Sci. 602, 156-161), while the expressions from Johnson et al. fit the data best at higher energies (Johnson, RE., Burger, M.H., Cassidy, T.A., Leblanc, F., Marconi, M., Smyth, W.H., 2009. Composition and Detection of Europa's Sputter-Induced Atmosphere, in: Pappalardo, RT., McKinnon, W.B., Khurana, K.K. (Eds.), Europa. University of Arizona Press, Tucson.). We compare the calculated sputtering rate with estimates of water ice regolith grain size as estimated from Galileo Near-Infrared Mapping Spectrometer (NIMS) data, and find that they are strongly correlated as previously suggested by Clark et al. (Clark, IN., Fanale, F.P., Zent, A.P., 1983. Frost grain size metamorphism: Implications for remote sensing of planetary surfaces. Icarus 56, 233-245.). The mechanism responsible for the sputtering rate/grain size link is uncertain. We also report a surface composition estimate using NIMS data from an area on the trailing hemisphere apex. We find a high abundance of sulfuric acid hydrate and radiation-resistant hydrated salts along with large water ice regolith grains, all of which are consistent with the high levels of magnetospheric bombardment at the trailing apex. (C) 2012 Elsevier Ltd. All rights reserved.
C1 [Cassidy, T. A.] Univ Colorado, Lab Atmospher & Space Phys, Boulder, CO 80303 USA.
[Paranicas, C. P.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA.
[Shirley, J. H.; Dalton, J. B., III; Kamp, L.; Hendrix, A. R.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Teolis, B. D.] SW Res Inst, Space Sci & Engn Div, San Antonio, TX 78238 USA.
[Johnson, R. E.] Univ Virginia, Charlottesville, VA 22904 USA.
RP Cassidy, TA (reprint author), Univ Colorado, Lab Atmospher & Space Phys, 1234 Discovery Dr, Boulder, CO 80303 USA.
EM timothy.cassidy@lasp.colorado.edu
RI Paranicas, Christopher/B-1470-2016
OI Paranicas, Christopher/0000-0002-4391-8255
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PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0032-0633
J9 PLANET SPACE SCI
JI Planet Space Sci.
PD MAR
PY 2013
VL 77
SI SI
BP 64
EP 73
DI 10.1016/j.pss.2012.07.008
PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 127PS
UT WOS:000317711500007
ER
PT J
AU Emmons, D
Acebal, A
Pulkkinen, A
Taktakishvili, A
MacNeice, P
Odstrcil, D
AF Emmons, D.
Acebal, A.
Pulkkinen, A.
Taktakishvili, A.
MacNeice, P.
Odstrcil, D.
TI Ensemble forecasting of coronal mass ejections using the WSA-ENLIL with
CONED Model
SO SPACE WEATHER-THE INTERNATIONAL JOURNAL OF RESEARCH AND APPLICATIONS
LA English
DT Article
ID DISTURBANCES; SIMULATION; CMES
AB The combination of the Wang-Sheeley-Arge (WSA) coronal model, ENLIL heliospherical model version 2.7, and CONED Model version 1.3 (WSA-ENLIL with CONED Model) was employed to form ensemble forecasts for 15 halo coronal mass ejections (halo CMEs). The input parameter distributions were formed from 100 sets of CME cone parameters derived from the CONED Model. The CONED Model used image processing along with the bootstrap approach to automatically calculate cone parameter distributions from SOHO/LASCO imagery based on techniques described by Pulkkinen et al. (2010). The input parameter distributions were used as input to WSA-ENLIL to calculate the temporal evolution of the CMEs, which were analyzed to determine the propagation times to the L-1 Lagrangian point and the maximum K-p indices due to the impact of the CMEs on the Earth's magnetosphere. The Newell et al. (2007) K-p index formula was employed to calculate the maximum K-p indices based on the predicted solar wind parameters near Earth assuming two magnetic field orientations: a completely southward magnetic field and a uniformly distributed clock-angle in the Newell et al. (2007) K-p index formula. The forecasts for 5 of the 15 events had accuracy such that the actual propagation time was within the ensemble average plus or minus one standard deviation. Using the completely southward magnetic field assumption, 10 of the 15 events contained the actual maximum K-p index within the range of the ensemble forecast, compared to 9 of the 15 events when using a uniformly distributed clock angle. Citation: Emmons, D., A. Acebal, A. Pulkkinen, A. Taktakishvili, P. MacNeice, and D. Odstrcil (2013), Ensemble forecasting of coronal mass ejections using the WSA-ENLIL with CONED Model, Space Weather, 11, 95-106, doi: 10.1002/swe.20019.
C1 [Emmons, D.; Acebal, A.] USAF, Dept Engn Phys, Inst Technol, Dayton, OH USA.
[Emmons, D.] USAF, Res Lab, Space Vehicles Directorate, Albuquerque, NM 87116 USA.
[Pulkkinen, A.; Taktakishvili, A.; MacNeice, P.; Odstrcil, D.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Pulkkinen, A.] Catholic Univ Amer, Washington, DC 20064 USA.
[Odstrcil, D.] George Mason Univ, Fairfax, VA 22030 USA.
RP Emmons, D (reprint author), USAF, Res Lab, Space Vehicles Directorate, Albuquerque, NM 87116 USA.
EM emmons29@yahoo.com
FU Air Force Institute of Technology; Community Coordinated Modeling Center
FX This analysis was sponsored by the Air Force Institute of Technology and
the Community Coordinated Modeling Center. D. Emmons was sponsored by
the Air Force Institute of Technology. The authors would like to thank
NOAA/SWPC's warehouse, NASA's OMNIWeb and CDAW data centers, and the
CELIAS/MTOF Proton Monitor (http://umtof.umd.edu/pm/) for the use of
their data. The views expressed in this article are those of the authors
and do not necessarily reflect the official policy or position of the
Air Force, the Department of Defense, or the U. S. government.
NR 23
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PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 1542-7390
J9 SPACE WEATHER
JI Space Weather
PD MAR
PY 2013
VL 11
IS 3
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DI 10.1002/swe.20019
PG 12
WC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology &
Atmospheric Sciences
SC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology &
Atmospheric Sciences
GA 129JC
UT WOS:000317834300003
ER
PT J
AU Ngwira, CM
Pulkkinen, A
Wilder, FD
Crowley, G
AF Ngwira, Chigomezyo M.
Pulkkinen, Antti
Wilder, Frederick D.
Crowley, Geoffrey
TI Extended study of extreme geoelectric field event scenarios for
geomagnetically induced current applications
SO SPACE WEATHER-THE INTERNATIONAL JOURNAL OF RESEARCH AND APPLICATIONS
LA English
DT Article
ID PLANETARY MAGNETIC-FIELD; ELECTRIC-FIELDS; POWER-SYSTEM; OCTOBER 2003;
STORM; IONOSPHERE; SUBSTORM; MAGNETOSPHERE; EXPANSION
AB Geomagnetically induced currents (GIC) flowing in man-made ground technological systems are a direct manifestation of adverse space weather. Today, there is great concern over possible geomagnetically induced current effects on power transmission networks that can result from extreme space weather events. The threat of severe societal consequences has accelerated recent interest in extreme geomagnetic storm impacts on high-voltage power transmission systems. As a result, extreme geomagnetic event characterization is of fundamental importance for quantifying the technological impacts and societal consequences of extreme space weather. This article reports on the global behavior of the horizontal geomagnetic field and the induced geoelectric field fluctuations during severe/extreme geomagnetic events. This includes (1) an investigation of the latitude threshold boundary, (2) the local time dependency of the maximum induced geoelectric field, and (3) the influence of the equatorial electrojet (EEJ) current on the occurrence of enhanced induced geoelectric fields over ground stations located near the dip equator. Using ground-based and satellite-borne Defense Meteorological Satellite Program measurements, this article confirms that the latitude threshold boundary is associated with the movements of the auroral oval and the corresponding auroral electrojet current system, which is the main driver of the largest perturbations of the ground geomagnetic field at high latitudes. In addition, we show that the enhancement of the EEJ is driven by the penetration of high-latitude electric fields and that the induced geoelectric fields at stations within the EEJ belt can be an order of magnitude larger than that at stations outside the belt. This has important implications for power networks located around the electrojet belt and confirms that earlier observations by Pulkkinen et al. (2012) were not isolated incidences but rather cases that can occur during certain severe geomagnetic storm events. Citation: Ngwira, C. M., A. Pulkkinen, F. D. Wilder, and G. Crowley (2013), Extended study of extreme geoelectric field event scenarios for geomagnetically induced current applications, Space Weather, 11, 121-131, doi:10.1002/swe.20021.
C1 [Ngwira, Chigomezyo M.; Pulkkinen, Antti] Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA.
[Ngwira, Chigomezyo M.; Pulkkinen, Antti] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Wilder, Frederick D.] Univ Colorado, Atmospher & Space Phys Lab, Boulder, CO 80309 USA.
[Wilder, Frederick D.; Crowley, Geoffrey] Atmospher & Space Technol Res Associates, Boulder, CO USA.
RP Ngwira, CM (reprint author), Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA.
EM chigongwira@yahoo.co.uk
RI ngwira, chigomezyo/D-7310-2012
FU EPRI [EPRI-18403]; National Science Foundation Atmospheric and Geospace
Sciences Postdoctoral Research Fellowshi
FX All the ground-based geomagnetic data used for this study was downloaded
through INTERMAGNET. We thank INTERMAGNET for promoting high standards
of observatory practice. The DMSP particle detectors were designed by
Dave Hardy of AFRL and data obtained from NOAA NGDC, and the DMSP
thermal plasma data are provided by the Center for Space Science at
University of Texas at Dallas. The authors thank the WDC-Kyoto team for
the auroral region data. The solar wind data were accessed through the
CDAWeb database, which is hosted by the NASA-GSFC Space Physics Data
Facility. The research work of C. M. Ngwira is supported by EPRI under
contract EPRI-18403. F. D. Wilder's efforts were supported by the
National Science Foundation Atmospheric and Geospace Sciences
Postdoctoral Research Fellowship.
NR 53
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PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 1539-4956
J9 SPACE WEATHER
JI Space Weather
PD MAR
PY 2013
VL 11
IS 3
BP 121
EP 131
DI 10.1002/swe.20021
PG 11
WC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology &
Atmospheric Sciences
SC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology &
Atmospheric Sciences
GA 129JC
UT WOS:000317834300005
ER
PT J
AU Braun, SA
Kakar, R
Zipser, E
Heymsfield, G
Albers, C
Brown, S
Durden, SL
Guimond, S
Halverson, J
Heymsfield, A
Ismail, S
Lambrigtsen, B
Miller, T
Tanelli, S
Thomas, J
Zawislak, J
AF Braun, Scott A.
Kakar, Ramesh
Zipser, Edward
Heymsfield, Gerald
Albers, Cerese
Brown, Shannon
Durden, Stephen L.
Guimond, Stephen
Halverson, Jeffery
Heymsfield, Andrew
Ismail, Syed
Lambrigtsen, Bjorn
Miller, Timothy
Tanelli, Simone
Thomas, Janel
Zawislak, Jon
TI NASA'S GENESIS AND RAPID INTENSIFICATION PROCESSES (GRIP) FIELD
EXPERIMENT
SO BULLETIN OF THE AMERICAN METEOROLOGICAL SOCIETY
LA English
DT Article
ID SAHARAN AIR LAYER; EYEWALL VERTICAL MOTION; TROPICAL CYCLOGENESIS; PART
II; CLOUD-SYSTEMS; WIND SHEAR; HURRICANES; INTENSITY; ATLANTIC;
EVOLUTION
AB In August-September 2010, NASA, NOAA, and the National Science Foundation (NSF) conducted separate but closely coordinated hurricane field campaigns, bringing to bear a combined seven aircraft with both new and mature observing technologies. NASA's Genesis and Rapid Intensification Processes (GRIP) experiment, the subject of this article, along with NOAA's Intensity Forecasting Experiment (IFEX) and NSF's Pre-Depression Investigation of Cloud-Systems in the Tropics (PREDICT) experiment, obtained unprecedented observations of the formation and intensification of tropical cyclones. The major goal of GRIP was to better understand the physical processes that control hurricane formation and intensity change, specifically the relative roles of environmental and inner-core processes. A key focus of GRIP was the application of new technologies to address this important scientific goal, including the first ever use of the unmanned Global Hawk aircraft for hurricane science operations. NASA and NOAA conducted coordinated flights to thoroughly sample the rapid intensification (RI) of Hurricanes Earl and Karl. The tri-agency aircraft teamed up to perform coordinated flights for the genesis of Hurricane Karl and Tropical Storm Matthew and the nonredevelopment of the remnants of Tropical Storm Gaston. The combined GRIP-IFEX-PREDICT datasets, along with remote sensing data from a variety of satellite platforms [Geostationary Operational Environmental Satellite (GOES), Tropical Rainfall Measuring Mission (TRMM), Aqua, Terra, CloudSat, and Cloud-Aerosol Lidar and Infrared Pathfinder Satellite Observations (CALIPSO)], will contribute to advancing understanding of hurricane formation and intensification. This article summarizes the GRIP experiment, the missions flown, and some preliminary findings.
C1 [Braun, Scott A.; Heymsfield, Gerald; Guimond, Stephen] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Kakar, Ramesh] NASA, Washington, DC 20546 USA.
[Zipser, Edward; Zawislak, Jon] Univ Utah, Salt Lake City, UT USA.
[Albers, Cerese] Florida State Univ, Tallahassee, FL 32306 USA.
[Brown, Shannon; Durden, Stephen L.; Lambrigtsen, Bjorn; Tanelli, Simone] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Guimond, Stephen] Oak Ridge Associated Univ, Oak Ridge, TN USA.
[Halverson, Jeffery; Thomas, Janel] Univ Maryland, Baltimore, MD 21201 USA.
[Heymsfield, Andrew] Natl Ctr Atmospher Res, Boulder, CO 80307 USA.
[Ismail, Syed] NASA, Langley Res Ctr, Hampton, VA 23665 USA.
[Miller, Timothy] NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA.
RP Braun, SA (reprint author), NASA, Goddard Space Flight Ctr, Code 612, Greenbelt, MD 20771 USA.
EM scott.a.braun@nasa.gov
RI Heymsfield, Andrew/E-7340-2011
FU National Aeronautics and Space Administration
FX The GRIP campaign owes its success to the hard work of many individuals
who served as mission scientists during the campaign, including John
Molinari, Elizabeth Ritchie, Robert Houze Jr., Greg McFarquhar, Richard
Blakeslee, and Michael Black. We also would like to thank Bruce
Anderson, Aaron Bansemer, Richard Blakeslee, Michael Goodman, Johnny
Hall, Svetla Hristova-Veleva, Doug Mach, Robert Rogers, Lin Tian, and
Luke Ziemba for their assistance with an earlier draft of the
manuscript, and Paul Newman at Goddard for his help in drafting Fig. 1.
A portion of this research (Brown, Durden, La mbrigtsen, and Tanelli)
was carried out at the Jet Propulsion Laboratory, California Institute
of Technology, under a contract with the National Aeronautics and Space
Administration.
NR 46
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PU AMER METEOROLOGICAL SOC
PI BOSTON
PA 45 BEACON ST, BOSTON, MA 02108-3693 USA
SN 0003-0007
J9 B AM METEOROL SOC
JI Bull. Amer. Meteorol. Soc.
PD MAR
PY 2013
VL 94
IS 3
BP 345
EP 363
DI 10.1175/BAMS-D-11-00232.1
PG 19
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 122OO
UT WOS:000317327600006
ER
PT J
AU Kucera, PA
Ebert, EE
Turk, FJ
Levizzani, V
Kirschbaum, D
Tapiador, FJ
Loew, A
Borsche, M
AF Kucera, Paul A.
Ebert, Elizabeth E.
Turk, F. Joseph
Levizzani, Vincenzo
Kirschbaum, Dalia
Tapiador, Francisco J.
Loew, Alexander
Borsche, M.
TI PRECIPITATION FROM SPACE Advancing Earth System Science
SO BULLETIN OF THE AMERICAN METEOROLOGICAL SOCIETY
LA English
DT Article
ID POTENTIAL TRAP TECHNIQUE; SATELLITE-OBSERVATIONS; PASSIVE MICROWAVE;
RAINFALL; VALIDATION; CLIMATE; TRMM; RESOLUTION; PRODUCTS; MISSION
AB Advances to space-based observing systems and data processing techniques have made precipitation datasets quickly and easily available via various data portals and widely used in Earth sciences. The increasingly lengthy time span of space-based precipitation data records has enabled cross-discipline investigations and applications that would otherwise not be possible, revealing discoveries related to hydrological and land processes, climate, atmospheric composition, and ocean freshwater budget and proving a vital element in addressing societal issues. The purpose of this article is to demonstrate how the availability and continuity of precipitation data records from recent and upcoming space missions is transforming the ways that scientific and societal issues are addressed, in ways that would not be otherwise possible.
C1 [Kucera, Paul A.] Natl Ctr Atmospher Res, Boulder, CO 80307 USA.
[Ebert, Elizabeth E.] Ctr Australian Weather & Climate Res, Bur Meteorol, Melbourne, Vic, Australia.
[Turk, F. Joseph] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Levizzani, Vincenzo] CNR, Inst Atmospher Sci & Climate, Bologna, Italy.
[Kirschbaum, Dalia] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Tapiador, Francisco J.] Univ Castilla La Mancha, Fac Environm Sci & Biochem, Toledo, Spain.
[Loew, Alexander; Borsche, M.] Max Planck Inst Meteorol, D-20146 Hamburg, Germany.
RP Kucera, PA (reprint author), Natl Ctr Atmospher Res, Res Applicat Lab, 3450 Mitchell Lane, Boulder, CO 80307 USA.
EM pkucera@ucar.edu
RI Levizzani, Vincenzo/A-9070-2013
OI Levizzani, Vincenzo/0000-0002-7620-5235
FU [PPII10-0162-5543]; [CGL2010-20787-C02-01]
FX This paper was facilitated through numerous discussions with
International Precipitation Working Group (IPWG; www.isac.cnr.it/similar
to ipwg/IPWG.html) members. We acknowledge Dr. Peng Xian from the Naval
Research Laboratory, Monterey for her assistance with the atmospheric
composition section. F. J. Tapiador acknowledges projects
PPII10-0162-5543 and CGL2010-20787-C02-01. This paper is dedicated to
David I. F. Grimes (1951-2011), who was an advocate for development and
outreach of precipitation products to meet societal needs in Africa.
NR 54
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PU AMER METEOROLOGICAL SOC
PI BOSTON
PA 45 BEACON ST, BOSTON, MA 02108-3693 USA
SN 0003-0007
J9 B AM METEOROL SOC
JI Bull. Amer. Meteorol. Soc.
PD MAR
PY 2013
VL 94
IS 3
BP 365
EP 375
DI 10.1175/BAMS-D-11-00171.1
PG 11
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 122OO
UT WOS:000317327600007
ER
PT J
AU Danowsky, B
Thompson, PM
Kukreja, S
AF Danowsky, Brian
Thompson, Peter M.
Kukreja, Sunil
TI Nonlinear Analysis of Aeroservoelastic Models with Free Play Using
Describing Functions
SO JOURNAL OF AIRCRAFT
LA English
DT Article; Proceedings Paper
CT 48th AIAA Aerospace Sciences Meeting and Exhibit / New Horizons Forum
and Aerospace Exposition
CY JAN 04-08, 2010
CL Orlando, FL
SP AIAA, Vinnova, Maritime Competence Ctr Lighthouse, Swedish Armed Forces, Swedish Def Mat Agcy, NASA Langley Res Ctr, NASA Dryden Flight Res Ctr
ID DOUBLET-LATTICE METHOD; IDENTIFICATION; FLOWS
AB DOI: 10.2514/1.C031370 Nonlinearities in aeroservoelastic systems are a source of limit-cycle oscillations. Aerodynamic control surfaces and actuators may have excessive free play in connecting joints and hinges, which has the potential to cause limit-cycle oscillations associated with aeroservoelastic vibrations, impacting handling and ride quality and leading to structural fatigue. Because of these negative impacts, free-play limits have been established by the Joint Services Guidance Military Specification. These military specifications have also been adopted by the Federal Aviation Administration for commercial aircraft. This stringent requirement can be excessively conservative and is very difficult and costly to meet. Analytical tools using describing functions have been developed to establish free-play limits on aeroservoelastic aircraft systems without adverse consequences. These tools are robust and easy to implement, justifying relaxation or validation of the conservative requirements. It is shown that oscillation frequency and amplitude can be accurately estimated using describing functions with an analytical model of an aeroservoelastic system with free play. A novel analysis technique is also demonstrated, whereby free-play occurrence and limit-cycle behavior can be visualized using time-varying frequency content. Validation of the method is illustrated with an aeroservoelastic stabilator control surface model using nonlinear simulation, with free-play limits found in experimental conditions.
C1 [Danowsky, Brian; Thompson, Peter M.] Syst Technol Inc, Hawthorne, CA 90250 USA.
[Kukreja, Sunil] NASA, Dryden Flight Res Ctr, Edwards AFB, CA 93560 USA.
RP Danowsky, B (reprint author), Syst Technol Inc, Hawthorne, CA 90250 USA.
NR 26
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U1 0
U2 5
PU AMER INST AERONAUTICS ASTRONAUTICS
PI RESTON
PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA
SN 0021-8669
J9 J AIRCRAFT
JI J. Aircr.
PD MAR-APR
PY 2013
VL 50
IS 2
BP 329
EP 336
DI 10.2514/1.C031370
PG 8
WC Engineering, Aerospace
SC Engineering
GA 122MJ
UT WOS:000317321900001
ER
PT J
AU Yoo, SY
AF Yoo, Seung Y.
TI Analysis of the Effects of Streamwise Lift Distribution on Sonic Boom
Signature
SO JOURNAL OF AIRCRAFT
LA English
DT Article; Proceedings Paper
CT 28th AIAA Applied Aerodynamics Conference
CY JUN 28-JUL 01, 2010
CL Chicago, IL
SP AIAA
AB DOI: 10.2514/1.C031517 The streamwise lift distribution of a wing-canard-stabilator-body model was varied to study its effect on the near-field sonic boom signature. The investigation was carried out via solving the three-dimensional Euler equation with the OVERFLOW-2 flow solver. The computational meshes were created using the Chimera overset grid topology. The lift distribution was varied by deflecting the canard, then trimming the aircraft with the wing and the stabilator while maintaining a constant lift coefficient of 0.05. A wide range of streamwise lift distributions was simulated. The results show that the relative longitudinal wave propagation speed can be controlled through lift distribution, thus controlling the shock coalescence and sonic boom signature. In addition, validation studies of the computational tools were performed using a wing-body model and the results were compared against the wind-tunnel experimental data. The same model was also used to perform the grid resolution and numerical scheme comparison study.
C1 NASA, Dryden Flight Res Ctr, Controls & Dynam Branch, Edwards AFB, CA 93523 USA.
RP Yoo, SY (reprint author), NASA, Dryden Flight Res Ctr, Controls & Dynam Branch, POB 273-MS 4840D, Edwards AFB, CA 93523 USA.
NR 23
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U1 0
U2 5
PU AMER INST AERONAUTICS ASTRONAUTICS
PI RESTON
PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA
SN 0021-8669
EI 1533-3868
J9 J AIRCRAFT
JI J. Aircr.
PD MAR-APR
PY 2013
VL 50
IS 2
BP 354
EP 359
DI 10.2514/1.C031517
PG 6
WC Engineering, Aerospace
SC Engineering
GA 122MJ
UT WOS:000317321900003
ER
PT J
AU Sitaraman, J
Potsdam, M
Wissink, A
Jayaraman, B
Datta, A
Mavriplis, D
Saberi, H
AF Sitaraman, Jayanarayanan
Potsdam, Mark
Wissink, Andrew
Jayaraman, Buvaneswari
Datta, Anubhav
Mavriplis, Dimitri
Saberi, Hossein
TI Rotor Loads Prediction Using Helios: A Multisolver Framework for
Rotorcraft Aeromechanics Analysis
SO JOURNAL OF AIRCRAFT
LA English
DT Article; Proceedings Paper
CT 49th AIAA Aerospace Sciences Meeting/New Horizons Forum and Aerospace
Exposition
CY JAN 03-17, 2011
CL Orlando, FL
SP AIAA
AB This paper documents the prediction of UH-60A Black Hawk aerodynamic loading using the multisolver Computational Fluid Dynamics/Computational Structural Dynamics analysis framework for rotorcraft Helios for a range of critical steady forward flight conditions. Comparisons with available flight test data are provided for all of the predictions. The Helios framework combines multiple solvers and multiple grid paradigms (unstructured and adaptive Cartesian) such that the advantages of each paradigm is preserved. Further, the software is highly automated for execution and designed in a modular fashion to minimize the burden on both the users and developers. The technical approach presented herein provides details of all of the participant modules and the interfaces used for their integration into the software framework. The results composed of sectional aerodynamic loading and wake visualizations are presented. Solution-based adapative mesh refinement, a salient feature of the Helios framework, is explored for all flight conditions and comparisons are provided for both aerodynamic loading and vortex wake structure with and without adaptive mesh refinement.
C1 [Sitaraman, Jayanarayanan; Mavriplis, Dimitri] Univ Wyoming, Dept Mech Engn, Laramie, WY 82071 USA.
[Potsdam, Mark] USA, Aeroflightdynam Directorate, Res Dev & Engn Command, Moffett Field, CA 94035 USA.
[Wissink, Andrew] USA, Aeroflightdynam Directorate, Sci & Technol Corp, Moffett Field, CA 94035 USA.
[Jayaraman, Buvaneswari; Datta, Anubhav] NASA, Ames Res Ctr, Sci & Technol Corp, Moffett Field, CA 94035 USA.
[Saberi, Hossein] Adv Rotorcraft Technol Inc, Sunnyvale, CA 94085 USA.
RP Sitaraman, J (reprint author), Univ Wyoming, Dept Mech Engn, Laramie, WY 82071 USA.
EM saberi@flightlab.com
NR 26
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U1 0
U2 3
PU AMER INST AERONAUTICS ASTRONAUTICS
PI RESTON
PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA
SN 0021-8669
J9 J AIRCRAFT
JI J. Aircr.
PD MAR-APR
PY 2013
VL 50
IS 2
BP 478
EP 492
DI 10.2514/1.C031897
PG 15
WC Engineering, Aerospace
SC Engineering
GA 122MJ
UT WOS:000317321900015
ER
PT J
AU Gracio, BJC
Pais, ARV
van Paassen, MM
Mulder, M
Kelly, LC
Houck, JA
AF Gracio, Bruno Jorge Correia
Pais, Ana Rita Valente
van Paassen, M. M. (Rene)
Mulder, Max
Kelly, Lon C.
Houck, Jacob A.
TI Optimal and Coherence Zone Comparison Within and Between Flight
Simulators
SO JOURNAL OF AIRCRAFT
LA English
DT Article; Proceedings Paper
CT AIAA Modeling and Simulation Technologies Conference
CY AUG 08-11, 2011
CL Portland, OR
SP AIAA
ID PERCEPTION; MOTION
AB In flight simulation, motion-cueing algorithms are used to transform aircraft motion into motion within the simulator limits. When looking for the best match between visual and inertial amplitude in a simulator, researchers have found that there is a range of inertial amplitudes, rather than a single inertial value, that is perceived by subjects as optimal. This zone, hereafter referred to as the optimal zone, seems to correlate to the perceptual coherence zones measured in flight simulators. However, no studies were found in which these two zones were compared. This study investigates the relation between the optimal and the coherence-zone measurements within and between different simulators. An experiment was conducted at NASA Langley Research Center, where two simulators were used to measure the optimal and the coherence zone in the sway axis. Results show that the optimal zone lies within the coherence zone. The center of the optimal zone is significantly lower than the center of the coherence zone. In addition, it was found that, whereas the width of the coherence zone depends on the visual amplitude and frequency, the width of the optimal zone remains constant. No statistical differences between the two simulators were found.
C1 [Gracio, Bruno Jorge Correia; Pais, Ana Rita Valente; van Paassen, M. M. (Rene); Mulder, Max] Delft Univ Technol, Fac Aerosp Engn, Control & Simulat Div, NL-2600 GB Delft, Netherlands.
[Kelly, Lon C.] NASA, Langley Res Ctr, Unisys Corp, Hampton, VA 23681 USA.
[Houck, Jacob A.] NASA, Langley Res Ctr, Simulat Dev & Anal Branch, Hampton, VA 23681 USA.
RP Gracio, BJC (reprint author), Delft Univ Technol, Fac Aerosp Engn, Control & Simulat Div, POB 5058, NL-2600 GB Delft, Netherlands.
EM B.J.CorreiaGracio@tudelft.nl; A.R.ValentePais@tudelft.nl;
M.M.vanPaassen@tudelft.nl; M.Mulder@tudelft.nl; Lon.C.Kelly@nasa.gov;
Jacob.A.Houck@nasa.gov
RI MULDER, Max/G-6727-2011; van Paassen, Marinus/C-3338-2012
OI MULDER, Max/0000-0002-0932-3979; van Paassen,
Marinus/0000-0003-4700-1222
NR 24
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U2 4
PU AMER INST AERONAUTICS ASTRONAUTICS
PI RESTON
PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA
SN 0021-8669
J9 J AIRCRAFT
JI J. Aircr.
PD MAR-APR
PY 2013
VL 50
IS 2
BP 493
EP 507
DI 10.2514/1.C031870
PG 15
WC Engineering, Aerospace
SC Engineering
GA 122MJ
UT WOS:000317321900016
ER
PT J
AU Yeo, H
AF Yeo, Hyeonsoo
TI Investigation of UH-60A Rotor Performance and Loads at High Advance
Ratios
SO JOURNAL OF AIRCRAFT
LA English
DT Article; Proceedings Paper
CT 68th Annual Forum of the American-Helicopter-Society
CY MAY 01-03, 2012
CL Fort Worth, TX
SP Amer Helicopter Soc
ID COMPREHENSIVE ANALYSIS; HELICOPTER ROTORS
AB Wind tunnel measurements of the performance, airloads, and structural loads of a full-scale UH-60A Black Hawk main rotor operating at high advance ratios (up to 1.0) are compared with calculations obtained using the comprehensive rotorcraft analysis Comprehensive Analytical Model of Rotorcraft Aerodynamics and Dynamics II to understand physics and quantify this comprehensive code's accuracy and reliability in the prediction of rotor performance and loads at high advance ratios. Detailed comparisons are made on rotor thrust, control angles, power, and section loads to illustrate and understand unique aeromechanics phenomena in this regime. The analysis correctly predicts the thrust reversal with collective at high advance ratios. Rotor induced plus profile power is also reasonably well predicted with proper modeling of the shank. Airloads and structural loads correlation is fair. A significant underprediction of 2-per-revolution structural loads is observed.
C1 USA, Aeroflightdynam Directorate AMRDEC, Ames Res Ctr, Res Dev & Engn Command, Moffett Field, CA 94035 USA.
RP Yeo, H (reprint author), USA, Aeroflightdynam Directorate AMRDEC, Ames Res Ctr, Res Dev & Engn Command, Moffett Field, CA 94035 USA.
EM hyeonsoo.yeo@us.army.mil
NR 31
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PU AMER INST AERONAUTICS ASTRONAUTICS
PI RESTON
PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA
SN 0021-8669
J9 J AIRCRAFT
JI J. Aircr.
PD MAR-APR
PY 2013
VL 50
IS 2
BP 576
EP 589
DI 10.2514/1.C031958
PG 14
WC Engineering, Aerospace
SC Engineering
GA 122MJ
UT WOS:000317321900023
ER
PT J
AU Gyekenyesi, A
AF Gyekenyesi, Andrew
TI Integrating nondestructive inspections with autonomic logistics and
structural health monitoring strategies for aeronautic systems
SO JOURNAL OF INTELLIGENT MATERIAL SYSTEMS AND STRUCTURES
LA English
DT Article
DE Autonomic structures; structural health monitoring; sensor
ID ACOUSTO-ULTRASONICS; DAMAGE
AB In recent years, there has been much activity concerning health management of aviation systems. Many government-and industry-based research projects/programs are focused on integrated vehicle health management strategies that include sensor development for automated or manual fault detection, diagnostics, prognostics to define remaining useful life, as well as mitigation plans for continued safe operation during a fault. The overall objectives for such activities include increased safety as well as efficient and economic operation of an aircraft fleet. Currently, to assess structural faults, visual inspections and/or nondestructive inspection techniques are utilized as a required routine for certain design and life management strategies. The inspections are manually involved and are carried out during aircraft downtime (e. g. on the runway or nightly hangar maintenance) or during a more extensive aircraft overhaul. Even with the potential of automated structural health monitoring within an integrated vehicle health management system, it is foreseen that manual and nondestructive inspections will continue to be an integral part of fleet life management. This article addresses and clarifies the role of nondestructive inspections in aircraft life management and its potential inclusion in future integrated vehicle health management systems.
C1 NASA Glenn Res Ctr Lewis Field, Ohio Aerosp Inst, Cleveland, OH 44135 USA.
RP Gyekenyesi, A (reprint author), NASA Glenn Res Ctr Lewis Field, Ohio Aerosp Inst, 21000 Brookpk Rd,MS 6-1, Cleveland, OH 44135 USA.
EM andrew.l.gyekenyesi@nasa.gov
FU NASA Glenn Research Center at Lewis Field; Vehicle Systems Safety
Technologies Project (Aviation Safety Program) under NASA [NNC07BA13B]
FX This study was supported by the NASA Glenn Research Center at Lewis
Field and the Vehicle Systems Safety Technologies Project (Aviation
Safety Program) under NASA Contract Number-NNC07BA13B.
NR 35
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PU SAGE PUBLICATIONS LTD
PI LONDON
PA 1 OLIVERS YARD, 55 CITY ROAD, LONDON EC1Y 1SP, ENGLAND
SN 1045-389X
J9 J INTEL MAT SYST STR
JI J. Intell. Mater. Syst. Struct.
PD MAR
PY 2013
VL 24
IS 5
BP 574
EP 583
DI 10.1177/1045389X12464281
PG 10
WC Materials Science, Multidisciplinary
SC Materials Science
GA 126NW
UT WOS:000317625600005
ER
PT J
AU Milos, FS
Chen, YK
AF Milos, F. S.
Chen, Y. -K.
TI Ablation Predictions for Carbonaceous Materials Using Two Databases for
Species Thermodynamics
SO JOURNAL OF SPACECRAFT AND ROCKETS
LA English
DT Article; Proceedings Paper
CT 42nd AIAA Thermophysics Conference
CY JUN 27-30, 2011
CL Honolulu, HI
SP AIAA, NASA Ames Res Ctr (ARC), NASA Strateg Capabilities Assests Program
AB During previous work at NASA Ames Research Center, most ablation predictions were obtained using a species thermodynamics database derived primarily from the JANAF thermochemical tables. However, the chemical equilibrium with applications thermodynamics database, also used by NASA, is considered more up to date. In this work, ablation analyses were performed for carbon and carbon phenolic materials using both sets of species thermodynamics. The ablation predictions are comparable at low and moderate heat fluxes, where the dominant mechanism is carbon oxidation. For high heat fluxes where sublimation is important, the predictions differ, with the chemical equilibrium with applications model predicting a lower ablation rate. The disagreement is greater for carbon phenolic than for carbon, and this difference is attributed to hydrocarbon species that may contribute to the ablation rate. Sample calculations for representative Orion and Stardust environments show significant differences only in the sublimation regime. For Stardust, if the calculations include a nominal environmental uncertainty for aeroheating, then the chemical equilibrium with applications model predicts a range of recession that is consistent with measurements for both heatshield cores.
C1 [Milos, F. S.; Chen, Y. -K.] NASA, Ames Res Ctr, Thermal Protect Mat Branch, Moffett Field, CA 94035 USA.
RP Milos, FS (reprint author), NASA, Ames Res Ctr, Thermal Protect Mat Branch, MS 234-1, Moffett Field, CA 94035 USA.
NR 18
TC 0
Z9 0
U1 1
U2 4
PU AMER INST AERONAUTICS ASTRONAUTICS
PI RESTON
PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA
SN 0022-4650
J9 J SPACECRAFT ROCKETS
JI J. Spacecr. Rockets
PD MAR-APR
PY 2013
VL 50
IS 2
BP 245
EP 255
DI 10.2514/1.A32316
PG 11
WC Engineering, Aerospace
SC Engineering
GA 121PY
UT WOS:000317257900001
ER
PT J
AU Chen, YK
Milos, FS
AF Chen, Yih-Kanq
Milos, Frank S.
TI Effects of Nonequilibrium Chemistry and Darcy-Forchheimer Pyrolysis Flow
for Charring Ablator
SO JOURNAL OF SPACECRAFT AND ROCKETS
LA English
DT Article; Proceedings Paper
CT 42nd AIAA Thermophysics Conference
CY JUN 27-30, 2011
CL Honolulu, HI
SP AIAA, NASA Ames Res Ctr (ARC), NASA Strateg Capabilities Assests Program
ID THERMAL RESPONSE; GAS; PERMEABILITY; PROGRAM; MODEL
AB The fully implicit ablation and thermal response code simulates pyrolysis and ablation of thermal protection materials and systems. The governing equations, which include energy conservation, a three-component decomposition model, and a surface energy balance, are solved with a moving grid. This work describes new modeling capabilities that are added to a special version of code. These capabilities include a time-dependent pyrolysis gas flow momentum equation with Darcy-Forchheimer terms and pyrolysis gas species conservation equations with finite-rate homogeneous chemical reactions. The total energy conservation equation is also enhanced for consistency with these new additions. Two groups of parametric studies of the phenolic impregnated carbon ablator are performed. In the first group, an Orion flight environment for a proposed lunar-return trajectory is considered. In the second group, various test conditions for arcjet models are examined. The central focus of these parametric studies is to understand the effect of pyrolysis gas momentum transfer on material in-depth thermal responses with finite-rate, equilibrium, or frozen homogeneous gas chemistry. Results indicate that the presence of chemical nonequilibrium pyrolysis gas flow does not significantly alter the in-depth thermal response performance predicted using the chemical equilibrium gas model.
C1 [Chen, Yih-Kanq] NASA, Ames Res Ctr, Aerothermodynam Branch, Moffett Field, CA 94035 USA.
[Milos, Frank S.] NASA, Ames Res Ctr, Thermal Protect Mat Branch, Moffett Field, CA 94035 USA.
RP Chen, YK (reprint author), NASA, Ames Res Ctr, Aerothermodynam Branch, MS 230-2, Moffett Field, CA 94035 USA.
NR 18
TC 2
Z9 2
U1 1
U2 10
PU AMER INST AERONAUTICS ASTRONAUTICS
PI RESTON
PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA
SN 0022-4650
J9 J SPACECRAFT ROCKETS
JI J. Spacecr. Rockets
PD MAR-APR
PY 2013
VL 50
IS 2
BP 256
EP 269
DI 10.2514/1.A32289
PG 14
WC Engineering, Aerospace
SC Engineering
GA 121PY
UT WOS:000317257900002
ER
PT J
AU Mazaheri, A
AF Mazaheri, Alireza
TI High-Energy Atmospheric Reentry Test Aerothermodynamic Analysis
SO JOURNAL OF SPACECRAFT AND ROCKETS
LA English
DT Article
AB The aerothermodynamic environment around an 8.3 m High-Energy Atmospheric Reentry Test vehicle is assessed. Twelve nose-shape configurations are generated, and their responses at the peak heating trajectory point are compared against the baseline nose shape. The possibility of a two-piece thermal protection system design at the nose is also considered, as are the surface catalytic affects of the aeroheating environment of such a configuration. Based on these analyses, an optimum nose shape is proposed to minimize the surface heating. The heat flux sensitivity of the optimum geometry to the angle of attack variations are also studied. A recommendation is also made for a two-piece thermal protection system design, for which the surface catalytic uncertainty associated with the jump in heating at the nose-inflatable aerodynamic decelerator juncture is reduced by a minimum of 93%. In this paper, the aeroshell is assumed to be rigid, and the inflatable fluid interaction effect is left for future investigations.
C1 NASA, Langley Res Ctr, Aerothermodynam Branch, Hampton, VA 23681 USA.
RP Mazaheri, A (reprint author), NASA, Langley Res Ctr, Aerothermodynam Branch, M-S 408A, Hampton, VA 23681 USA.
EM Ali.R.Mazaheri@nasa.gov
FU hypersonic inflatable aerodynamic decelerators program; High-Energy
Atmospheric Reentry Test project
FX The author would like to thank the hypersonic inflatable aerodynamic
decelerators program and the High-Energy Atmospheric Reentry Test
project for supporting this work. The thanks would also go to the entire
High-Energy Atmospheric Reentry Test group for many good discussions on
this effort.
NR 17
TC 0
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U1 0
U2 10
PU AMER INST AERONAUTICS ASTRONAUTICS
PI RESTON
PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA
SN 0022-4650
J9 J SPACECRAFT ROCKETS
JI J. Spacecr. Rockets
PD MAR-APR
PY 2013
VL 50
IS 2
BP 270
EP 281
DI 10.2514/1.A32407
PG 12
WC Engineering, Aerospace
SC Engineering
GA 121PY
UT WOS:000317257900003
ER
PT J
AU Lee, AY
Wang, EK
Pilinski, EB
Macala, GA
Feldman, AW
AF Lee, Allan Y.
Wang, Eric K.
Pilinski, Emily B.
Macala, Glenn A.
Feldman, Antonette W.
TI Estimation and Modeling of Enceladus Plume Jet Density Using Cassini
Flight Data
SO JOURNAL OF SPACECRAFT AND ROCKETS
LA English
DT Article; Proceedings Paper
CT AIAA Guidance, Navigation, and Control Conference
CY AUG 02-06, 2010
CL Toronto, CANADA
SP Amer Inst Aeronaut & Astronaut (AIAA)
AB After an interplanetary cruise of almost seven years, the Cassini spacecraft arrived at Saturn on 30 June 2004. In 2005, Cassini completed three flybys of Enceladus, a small icy satellite of Saturn. Observations made during these flybys confirmed the existence of water vapor plumes in the south polar region of Enceladus. During an Enceladus flyby, plume jets imparted on the spacecraft resulted in small but visible attitude control errors. Using the known and unique transfer function between the disturbance torque and the attitude control error, the disturbance torque could be estimated. Furthermore, given good estimates of the spacecraft's projected area, center of pressure location, and spacecraft velocity, the time history of the Enceladus plume density could be reconstructed. Next, the density due to each plume jet as a function of both the radial distance of the spacecraft from the plume source and the angular distance of the spacecraft from the axis of symmetry of the jet was modeled. By comparing the reconstructed plume density with that predicted by the plume model, values of the plume model parameters are determined. The validity of this plume density model is confirmed using flight data obtained from four low-altitude flybys of Enceladus in 2008-2011.
C1 [Lee, Allan Y.; Macala, Glenn A.] CALTECH, Jet Prop Lab, Guidance & Control Sect, Pasadena, CA 91109 USA.
[Wang, Eric K.] CALTECH, Jet Prop Lab, Guidance & Control Flight Software Validat Sect, Pasadena, CA 91109 USA.
[Pilinski, Emily B.] Univ Colorado, Lab Atmospher & Space Phys, Boulder, CO 80309 USA.
[Feldman, Antonette W.] CALTECH, Jet Prop Lab, Flight Engn Sect, Pasadena, CA 91109 USA.
RP Lee, AY (reprint author), CALTECH, Jet Prop Lab, Guidance & Control Sect, Mail Stop 230-104,4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM Allan.Y.Lee@jpl.nasa.gov; Erik.K.Wang@jpl.nasa.gov;
Emily.Pilinski@lasp.colorado.edu; Glenn.A.Macala@jpl.nasa.gov;
Antonette.W.Feldman@jpl.nasa.gov
NR 19
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U1 0
U2 11
PU AMER INST AERONAUTICS ASTRONAUTICS
PI RESTON
PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA
SN 0022-4650
J9 J SPACECRAFT ROCKETS
JI J. Spacecr. Rockets
PD MAR-APR
PY 2013
VL 50
IS 2
BP 317
EP 325
DI 10.2514/1.A32344
PG 9
WC Engineering, Aerospace
SC Engineering
GA 121PY
UT WOS:000317257900007
ER
PT J
AU Schonberg, W
Evans, S
Bjorkman, MD
AF Schonberg, William
Evans, Steve
Bjorkman, Michael D.
TI Hypervelocity Impact Testing of Multiwall Targets Using Multiple
Simultaneously Launched Projectiles
SO JOURNAL OF SPACECRAFT AND ROCKETS
LA English
DT Article
ID EQUATIONS; FACILITY
AB Multiwall shield designs for spacecraft have been studied extensively in the last four decades as a means of reducing the perforation threat of the near-Earth particulate environment over equivalent single-wall structures. The performance of an impact shield is typically characterized by its ballistic limit equation, which is obtained through high-speed impact tests that typically use spherical projectiles fired in light gas guns. Traditional firings employ only one projectile per launch package. However, some facilities have taken to launching multiple projectiles of different sizes in a single launch package. In light of the significant role played by a ballistic limit equation in risk assessment, a study was performed to examine whether or not this method of simultaneously launching several projectiles at a single target could give rise to some issues which may compromise the impact test data obtained in this manner. It was found that interference between debris clouds created by the impacting (simultaneously launched) particles could indeed occur. This in turn could affect the damage levels caused by the impacting particles as compared to those that would be seen in more standard single-projectile impact tests under the same impact conditions.
C1 [Schonberg, William] Missouri Univ Sci & Technol, Rolla, MO 65409 USA.
[Evans, Steve] NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA.
[Bjorkman, Michael D.] Jacobs Technol, Houston, TX 77058 USA.
RP Schonberg, W (reprint author), Missouri Univ Sci & Technol, Rolla, MO 65409 USA.
EM wschon@mst.edu
FU NASA Engineering Safety Center
FX The authors would like to acknowledge the support of the NASA
Engineering Safety Center for providing the support that made this study
possible.
NR 13
TC 0
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U1 1
U2 3
PU AMER INST AERONAUTICS ASTRONAUTICS
PI RESTON
PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA
SN 0022-4650
J9 J SPACECRAFT ROCKETS
JI J. Spacecr. Rockets
PD MAR-APR
PY 2013
VL 50
IS 2
BP 358
EP 364
DI 10.2514/1.A32118
PG 7
WC Engineering, Aerospace
SC Engineering
GA 121PY
UT WOS:000317257900012
ER
PT J
AU Stephens, JP
Vos, GA
Bilimoria, KD
Mueller, ER
Brazzel, J
Spehar, P
AF Stephens, John-Paul
Vos, Gordon A.
Bilimoria, Karl D.
Mueller, Eric R.
Brazzel, Jack
Spehar, Pete
TI Orion Handling Qualities During International Space Station Proximity
Operations and Docking
SO JOURNAL OF SPACECRAFT AND ROCKETS
LA English
DT Article; Proceedings Paper
CT AIAA Guidance, Navigation, and Control Conference
CY AUG 07-13, 2011
CL Portland, OR
SP AIAA
AB The Orion spacecraft is designed to automatically rendezvous and dock with many vehicles, including the International Space Station. However, the crew is able to assume manual control of the vehicle's attitude and flight path. In these instances, Orion must meet handling-qualities requirements established by NASA. Two handling. qualities assessments were conducted to evaluate preliminary designs of the vehicle using a six-degree-of-freedom, high-fidelity guidance, navigation, and control simulation. The first assessed Orion's handling qualities during the last 20 ft before docking and included both steady and oscillatory motions of the docking target. The second focused on manual acquisition of the docking axis during the proximity operations phase and subsequent station keeping. Cooper Harper handling-qualities ratings, workload ratings, and comments were provided by 10 evaluation pilots for the docking study and five evaluation pilots for the proximity operations study. For the docking task, both cases received 90% level 1 (satisfactory) handling-qualities ratings, exceeding the requirement. All ratings for the proximity operations task were level 1. These evaluations indicate that Orion is on course to meet its handling-qualities requirements for proximity operations and docking.
C1 [Stephens, John-Paul] Lockheed Martin, Explorat & Sci Solut, Houston, TX 77058 USA.
[Vos, Gordon A.] Wyle, Houston, TX 77058 USA.
[Bilimoria, Karl D.; Mueller, Eric R.] NASA, Ames Res Ctr, Flight Trajectory Dynam & Control Branch, Moffett Field, CA 94035 USA.
[Brazzel, Jack; Spehar, Pete] NASA, Lyndon B Johnson Space Ctr, Guidance Nav & Control Autonomous Flight Syst Bra, Houston, TX 77058 USA.
RP Stephens, JP (reprint author), Covidien, 5920 Longbow Dr,Mail Stop A23, Boulder, CO 80301 USA.
NR 26
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U1 0
U2 8
PU AMER INST AERONAUTICS ASTRONAUTICS
PI RESTON
PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA
SN 0022-4650
J9 J SPACECRAFT ROCKETS
JI J. Spacecr. Rockets
PD MAR-APR
PY 2013
VL 50
IS 2
BP 449
EP 457
DI 10.2514/1.A32253
PG 9
WC Engineering, Aerospace
SC Engineering
GA 121PY
UT WOS:000317257900021
ER
PT J
AU Mazaheri, A
AF Mazaheri, Alireza
TI Multispecies Reacting Characteristic Boundary Condition Implementation
with Applications
SO JOURNAL OF SPACECRAFT AND ROCKETS
LA English
DT Article
C1 NASA, Langley Res Ctr, Aerothermodynam Branch, Hampton, VA 23681 USA.
RP Mazaheri, A (reprint author), NASA, Langley Res Ctr, Aerothermodynam Branch, M-S 408A, Hampton, VA 23681 USA.
EM ali.r.mazaheri@nasa.gov
NR 12
TC 0
Z9 0
U1 0
U2 0
PU AMER INST AERONAUTICS ASTRONAUTICS
PI RESTON
PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA
SN 0022-4650
J9 J SPACECRAFT ROCKETS
JI J. Spacecr. Rockets
PD MAR-APR
PY 2013
VL 50
IS 2
BP 467
EP 470
DI 10.2514/1.A32136
PG 4
WC Engineering, Aerospace
SC Engineering
GA 121PY
UT WOS:000317257900025
ER
PT J
AU Burton, AS
Elsila, JE
Hein, JE
Glavin, DP
Dworkin, JP
AF Burton, Aaron S.
Elsila, Jamie E.
Hein, Jason E.
Glavin, Daniel P.
Dworkin, Jason P.
TI Extraterrestrial amino acids identified in metal-rich CH and CB
carbonaceous chondrites from Antarctica
SO METEORITICS & PLANETARY SCIENCE
LA English
DT Article
ID TAGISH LAKE METEORITE; MURCHISON METEORITE; ENANTIOMERIC EXCESSES; MASS
SPECTROMETRY; ORGANIC-COMPOUNDS; PARENT BODY; NUCLEOBASES; MOLECULES;
CHEMISTRY; EVOLUTION
AB Carbonaceous chondrites contain numerous indigenous organic compounds and could have been an important source of prebiotic compounds required for the origin of life on Earth or elsewhere. Extraterrestrial amino acids have been reported in five of the eight groups of carbonaceous chondrites and are most abundant in CI, CM, and CR chondrites but are also present in the more thermally altered CV and CO chondrites. We report the abundance, distribution, and enantiomeric and isotopic compositions of simple primary amino acids in six metal-rich CH and CB carbonaceous chondrites that have not previously been investigated for amino acids: Allan Hills (ALH) 85085 (CH3), Pecora Escarpment (PCA) 91467 (CH3), Patuxent Range (PAT) 91546 (CH3), MacAlpine Hills (MAC) 02675 (CBb), Miller Range (MIL) 05082 (CB), and Miller Range (MIL) 07411 (CB). Amino acid abundances and carbon isotopic values were obtained by using both liquid chromatography time-of-flight mass spectrometry and fluorescence, and gas chromatography isotope ratio mass spectrometry. The 13C/12C ratios of multiple amino acids fall outside of the terrestrial range and support their extraterrestrial origin. Extracts of CH chondrites were found to be particularly rich in amino acids (1316 parts per million, ppm) while CB chondrite extracts had much lower abundances (0.22 ppm). The amino acid distributions of the CH and CB chondrites were distinct from the distributions observed in type 2 and 3 CM and CR chondrites and contained elevated levels of -, -, and -amino acids compared to the corresponding -amino acids, providing evidence that multiple amino acid formation mechanisms were important in CH and CB chondrites.
C1 [Burton, Aaron S.] Catholic Univ Amer, Greenbelt, MD 20771 USA.
[Elsila, Jamie E.; Glavin, Daniel P.; Dworkin, Jason P.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Elsila, Jamie E.; Glavin, Daniel P.; Dworkin, Jason P.] Goddard Ctr Astrobiol, Greenbelt, MD 20771 USA.
[Hein, Jason E.] Univ Calif Merced, Sch Nat Sci, Dept Chem, Merced, CA 95343 USA.
RP Burton, AS (reprint author), Catholic Univ Amer, Greenbelt, MD 20771 USA.
EM aaron.s.burton@nasa.gov
RI Burton, Aaron/H-2212-2011; Elsila, Jamie/C-9952-2012; Glavin,
Daniel/D-6194-2012; Dworkin, Jason/C-9417-2012
OI Burton, Aaron/0000-0002-7137-1605; Glavin, Daniel/0000-0001-7779-7765;
Dworkin, Jason/0000-0002-3961-8997
FU National Aeronautics and Space Administration (NASA) Astrobiology
Institute; Goddard Center for Astrobiology; NASA
FX A. S. B. was supported by a NASA Postdoctoral Program fellowship
administered by Oak Ridge Associated Universities through a contract
with NASA. J. E. E., M. P. C., D. P. G., and J. P. D. acknowledge
funding support from the National Aeronautics and Space Administration
(NASA) Astrobiology Institute and the Goddard Center for Astrobiology
and the NASA Cosmochemistry and Exobiology Programs. We thank M.
Callahan and M. Martin for technical assistance; J. Aponte for helpful
discussions; M. Zolensky and an anonymous reviewer for insightful
reviews; and are grateful to ANSMET, K. Righter, and the members of the
Meteorite Working Group for allocating the meteorite samples analyzed in
this study.
NR 44
TC 22
Z9 23
U1 4
U2 30
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 1086-9379
J9 METEORIT PLANET SCI
JI Meteorit. Planet. Sci.
PD MAR
PY 2013
VL 48
IS 3
BP 390
EP 402
DI 10.1111/maps.12063
PG 13
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 117OP
UT WOS:000316963200005
ER
PT J
AU Galante, D
Rodrigues, F
Lima, IGP
Duarte, RTD
AF Galante, Douglas
Rodrigues, Fabio
Lima, Ivan Glaucio Paulino
Duarte, Rubens T. D.
CA SPASA Organizers
TI Research Focus Group Activity of the Sao Paulo Advanced School of
Astrobiology: SPASA 2011
SO ASTROBIOLOGY
LA English
DT Editorial Material
C1 [Galante, Douglas] Univ Sao Paulo, Inst Astron Geophys & Atmospher Sci, BR-05508090 Sao Paulo, Brazil.
[Galante, Douglas] Natl Ctr Res Energy & Mat, Brazilian Synchrotron Light Lab, Campinas, SP, Brazil.
[Rodrigues, Fabio] Univ Sao Paulo, Inst Chem, BR-05508090 Sao Paulo, Brazil.
[Lima, Ivan Glaucio Paulino] NASA, Ames Res Ctr, Div Earth Sci, Moffett Field, CA 94035 USA.
[Duarte, Rubens T. D.] Univ Sao Paulo, Oceanog Inst, BR-05508090 Sao Paulo, Brazil.
RP Galante, D (reprint author), Univ Sao Paulo, Inst Astron Geofis & Ciencias Atmosfer, Dept Astron, Rua Matao 1226, BR-05508090 Sao Paulo, Brazil.
EM douglasgalante@gmail.com
RI Duarte, Rubens/E-3129-2012; Institute of Chemistry - USP, Dept. of
Chemistry/B-8988-2012; Galante, Douglas/G-8752-2011
OI Galante, Douglas/0000-0002-3265-2527
NR 3
TC 0
Z9 0
U1 0
U2 5
PU MARY ANN LIEBERT INC
PI NEW ROCHELLE
PA 140 HUGUENOT STREET, 3RD FL, NEW ROCHELLE, NY 10801 USA
SN 1531-1074
J9 ASTROBIOLOGY
JI Astrobiology
PD MAR
PY 2013
VL 13
IS 3
BP 292
EP 293
DI 10.1089/ast.2013.0987
PG 2
WC Astronomy & Astrophysics; Biology; Geosciences, Multidisciplinary
SC Astronomy & Astrophysics; Life Sciences & Biomedicine - Other Topics;
Geology
GA 116CV
UT WOS:000316861100006
PM 23537138
ER
PT J
AU Barge, LM
Pulschen, AA
Emygdio, APM
Congreve, C
Kishimoto, DE
Bendia, AG
Teles, ADM
DeMarines, J
Stoupin, D
AF Barge, Laura M.
Pulschen, Andre A.
Mendes Emygdio, Ana Paula
Congreve, Curtis
Kishimoto, Dario E.
Bendia, Amanda G.
Teles, Antonio de Morais M.
DeMarines, Julia
Stoupin, Daniel
TI Life, the Universe, and Everything: An Education Outreach Proposal to
Build a Traveling Astrobiology Exhibit
SO ASTROBIOLOGY
LA English
DT Article
DE Museum; Traveling exhibit; Interactive display
AB Astrobiology is a transdisciplinary field with extraordinary potential for the scientific community. As such, it is important to educate the community at large about the growing importance of this field to increase awareness and scientific content learning and expose potential future scientists. To this end, we propose the creation of a traveling museum exhibit that focuses exclusively on astrobiology and utilizes modern museum exhibit technology and design. This exhibit (the "Astrobiology Road Show"), organized and evaluated by an international group of astrobiology students and postdocs, is planned to tour throughout the Americas.
C1 [Barge, Laura M.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Pulschen, Andre A.] Univ Fed Sao Carlos, Ctr Ciencias Agr, BR-13560 Sao Carlos, SP, Brazil.
[Mendes Emygdio, Ana Paula] Univ Estadual Paulista, Dept Educ, Inst Biociencias, Sao Paulo, Brazil.
[Congreve, Curtis] Univ Kansas, Dept Geol, Lawrence, KS 66045 USA.
[Kishimoto, Dario E.] Univ Buenos Aires, Fac Ciencias Exactas & Nat, Dept Biodiversidad & Biol Expt, Buenos Aires, DF, Argentina.
[Bendia, Amanda G.] Univ Fed Rio de Janeiro, Inst Biofis Carlos Chagas Filho, BR-21941 Rio De Janeiro, Brazil.
[Teles, Antonio de Morais M.] Brazilian Ctr Phys Res, Rio De Janeiro, Brazil.
[DeMarines, Julia] Denver Museum Nat & Sci, Dept Space Sci, Denver, CO USA.
[DeMarines, Julia] Blue Marble Space, Seattle, WA USA.
[Stoupin, Daniel] Russian Acad Sci, Inst Physicochem & Biol Problems Soil Sci, Pushchino 142292, Russia.
RP Barge, LM (reprint author), Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91107 USA.
EM laura.m.barge@jpl.nasa.gov
RI de Morais Teles, Antonio/G-4589-2013
OI de Morais Teles, Antonio/0000-0001-6104-0629
FU FAPESP (Sao Paulo Research Foundation); Universidade de Sao Paulo; NASA
Astrobiology Institute (Icy Worlds)
FX The authors thank FAPESP (Sao Paulo Research Foundation) and
Universidade de Sao Paulo for the financial support to attend the Sao
Paulo Advanced School of Astrobiology-SPASA 2011. Parts of the research
described in this publication were carried out at the Jet Propulsion
Laboratory, California Institute of Technology, under a contract with
the National Aeronautics and Space Administration with support by the
NASA Astrobiology Institute (Icy Worlds). (c) 2012. All rights reserved.
NR 12
TC 1
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U1 2
U2 10
PU MARY ANN LIEBERT INC
PI NEW ROCHELLE
PA 140 HUGUENOT STREET, 3RD FL, NEW ROCHELLE, NY 10801 USA
SN 1531-1074
J9 ASTROBIOLOGY
JI Astrobiology
PD MAR
PY 2013
VL 13
IS 3
BP 303
EP 308
DI 10.1089/ast.2012.0834
PG 6
WC Astronomy & Astrophysics; Biology; Geosciences, Multidisciplinary
SC Astronomy & Astrophysics; Life Sciences & Biomedicine - Other Topics;
Geology
GA 116CV
UT WOS:000316861100008
PM 23469863
ER
PT J
AU Acero, F
Gallant, Y
Ballet, J
Renaud, M
Terrier, R
AF Acero, F.
Gallant, Y.
Ballet, J.
Renaud, M.
Terrier, R.
TI A new nearby pulsar wind nebula overlapping the RX J0852.0-4622
supernova remnant
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE ISM: supernova remnants; pulsars: general; X-rays: individuals: RX
J0852.0-4622
ID GUM NEBULA; MOLECULAR CLOUDS; INTERSTELLAR GAS; STAR-FORMATION; DATA
RELEASE; XMM-NEWTON; X-RAYS; VELA; DISCOVERY; RX-J0852.0-4622
AB Context. Energetic pulsars can be embedded in a nebula of relativistic leptons that is powered by the dissipation of the rotational energy of the pulsar. The object PSRJ0855-4644 is an energetic and fast-spinning pulsar ((E) over dot = 1.1x10(36) erg s(-1), P = 65 ms) discovered near the southeast rim of the supernova remnant (SNR) RXJ0852.0-4622 (aka Vela Jr) by the Parkes multibeam survey. The position of the pulsar is in spatial coincidence with an enhancement in X-rays and TeV gamma-rays, which could be due to its putative pulsar wind nebula (PWN).
Aims. The purpose of this study is to search for diffuse non-thermal X-ray emission around PSRJ0855-4644 to test for the presence of a PWN and to estimate the distance to the pulsar.
Methods. An X-ray observation was carried out with the XMM-Newton satellite to constrain the properties of the pulsar and its nebula. The absorption column density derived in X-rays from the pulsar and from different regions of the SNR rim was compared with the absorption derived from the atomic (HI) and molecular ((CO)-C-12) gas distribution along the corresponding lines of sight to estimate the distance to the pulsar and to the SNR.
Results. The observation has revealed the X-ray counterpart of the pulsar together with surrounding extended emission, thus confirming the existence of a PWN. The comparison of column densities provided an upper limit to the distance to the pulsar PSRJ0855-4644 and the SNR RX J0852.0-4622 (d <= 900 pc). Although both objects are at compatible distances, we rule out that the pulsar and the SNR are associated. With this revised distance, PSRJ0855-4644 is the second most energetic pulsar, after the Vela pulsar, within a radius of 1 kpc and could therefore contribute to the local cosmic-ray e(-)/e(+) spectrum.
C1 [Acero, F.; Gallant, Y.; Renaud, M.] Univ Montpellier 2, CNRS, LUPM, F-34095 Montpellier 5, France.
[Acero, F.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Ballet, J.] Univ Paris 07, CNRS, CEA, AIM, F-75221 Paris 05, France.
[Terrier, R.] Univ Paris 07, APC, CNRS, F-75221 Paris 05, France.
RP Acero, F (reprint author), Univ Montpellier 2, CNRS, LUPM, F-34095 Montpellier 5, France.
EM facero@in2p3.fr
NR 39
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U1 1
U2 2
PU EDP SCIENCES S A
PI LES ULIS CEDEX A
PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A,
FRANCE
SN 0004-6361
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD MAR
PY 2013
VL 551
AR A7
DI 10.1051/0004-6361/201220799
PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 110QR
UT WOS:000316460600007
ER
PT J
AU Berta, S
Lutz, D
Santini, P
Wuyts, S
Rosario, D
Brisbin, D
Cooray, A
Franceschini, A
Gruppioni, C
Hatziminaoglou, E
Hwang, HS
Le Floc'h, E
Magnelli, B
Nordon, R
Oliver, S
Page, MJ
Popesso, P
Pozzetti, L
Pozzi, F
Riguccini, L
Rodighiero, G
Roseboom, I
Scott, D
Symeonidis, M
Valtchanov, I
Viero, M
Wang, L
AF Berta, S.
Lutz, D.
Santini, P.
Wuyts, S.
Rosario, D.
Brisbin, D.
Cooray, A.
Franceschini, A.
Gruppioni, C.
Hatziminaoglou, E.
Hwang, H. S.
Le Floc'h, E.
Magnelli, B.
Nordon, R.
Oliver, S.
Page, M. J.
Popesso, P.
Pozzetti, L.
Pozzi, F.
Riguccini, L.
Rodighiero, G.
Roseboom, I.
Scott, D.
Symeonidis, M.
Valtchanov, I.
Viero, M.
Wang, L.
TI Panchromatic spectral energy distributions of Herschel sources
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE infrared: galaxies; galaxies: statistics; galaxies: star formation;
galaxies: active; galaxies: evolution
ID ACTIVE GALACTIC NUCLEI; DEEP FIELD-SOUTH; STAR-FORMATION RATES;
FAR-INFRARED PROPERTIES; HIGH-REDSHIFT GALAXIES; MU-M OBSERVATIONS;
SIMILAR-TO 2.5; PHOTOMETRIC REDSHIFTS; GOODS-HERSCHEL; COSMOS FIELD
AB Combining far-infrared Herschel photometry from the PACS Evolutionary Probe (PEP) and Herschel Multi-tiered Extragalactic Survey (HerMES) guaranteed time programs with ancillary datasets in the GOODS-N, GOODS-S, and COSMOS fields, it is possible to sample the 8-500 mu m spectral energy distributions (SEDs) of galaxies with at least 7-10 bands. Extending to the UV, optical, and near-infrared, the number of bands increases up to 43. We reproduce the distribution of galaxies in a carefully selected restframe ten colors space, based on this rich data-set, using a superposition of multivariate Gaussian modes. We use this model to classify galaxies and build median SEDs of each class, which are then fitted with a modified version of the MAGPHYS code that combines stellar light, emission from dust heated by stars and a possible warm dust contribution heated by an active galactic nucleus (AGN). The color distribution of galaxies in each of the considered fields can be well described with the combination of 6-9 classes, spanning a large range of far- to near-infrared luminosity ratios, as well as different strength of the AGN contribution to bolometric luminosities. The defined Gaussian grouping is used to identify rare or odd sources. The zoology of outliers includes Herschel-detected ellipticals, very blue z similar to 1 Ly-break galaxies, quiescent spirals, and torus-dominated AGN with star formation. Out of these groups and outliers, a new template library is assembled, consisting of 32 SEDs describing the intrinsic scatter in the restframe UV-to-submm colors of infrared galaxies. This library is tested against L(IR) estimates with and without Herschel data included, and compared to eight other popular methods often adopted in the literature. When implementing Herschel photometry, these approaches produce L(IR) values consistent with each other within a median absolute deviation of 10-20%, the scatter being dominated more by fine tuning of the codes, rather than by the choice of SED templates. Finally, the library is used to classify 24 mu m detected sources in PEP GOODS fields on the basis of AGN content, L(60)/L(100) color and L(160)/L(1.6) luminosity ratio. AGN appear to be distributed in the stellar mass (M-*) vs. star formation rate (SFR) space along with all other galaxies, regardless of the amount of infrared luminosity they are powering, with the tendency to lie on the high SFR side of the "main sequence". The incidence of warmer star-forming sources grows for objects with higher specific star formation rates (sSFR), and they tend to populate the "off-sequence" region of the M-* - SFR - z space.
C1 [Berta, S.; Lutz, D.; Wuyts, S.; Rosario, D.; Magnelli, B.; Popesso, P.] Max Planck Inst Extraterr Phys MPE, D-85741 Garching, Germany.
[Santini, P.] INAF Osservatorio Astron Roma, I-00040 Monte Porzio Catone, Italy.
[Brisbin, D.] Cornell Univ, Ctr Radiophys & Space Res, Ithaca, NY 14853 USA.
[Cooray, A.] Univ Calif Irvine, Dept Phys & Astron, Irvine, CA 92697 USA.
[Franceschini, A.; Rodighiero, G.] Univ Padua, Dipartimento Astron, I-35122 Padua, Italy.
[Gruppioni, C.; Pozzetti, L.] INAF Osservatorio Astron Bologna, I-40127 Bologna, Italy.
[Hatziminaoglou, E.] ESO, D-85748 Garching, Germany.
[Hwang, H. S.] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA.
[Le Floc'h, E.] Univ Paris Diderot, IRFU Serv Astrophys, Lab AIM, CEA DSM,CNRS,CEA Saclay, F-91191 Gif Sur Yvette, France.
[Nordon, R.] Tel Aviv Univ, Raymond & Beverly Sackler Fac Exact Sci, Sch Phys & Astron, IL-69978 Tel Aviv, Israel.
[Oliver, S.; Wang, L.] Univ Sussex, Dept Phys & Astron, Ctr Astron, Brighton BN1 9QH, E Sussex, England.
[Page, M. J.; Symeonidis, M.] Univ Coll London, Mullard Space Sci Lab, Dorking RH5 6NT, Surrey, England.
[Pozzi, F.] Univ Bologna, Dipartimento Astron, I-40127 Bologna, Italy.
[Riguccini, L.] NASA, Astrophys Branch, Ames Res Ctr, Moffett Field, CA 94305 USA.
[Roseboom, I.] Univ Edinburgh, Inst Astron, Royal Observ, Edinburgh EH9 3HJ, Midlothian, Scotland.
[Scott, D.] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada.
[Valtchanov, I.] ESA, ESAC, Herschel Sci Ctr, Madrid 28691, Spain.
[Viero, M.] CALTECH, Pasadena, CA 91125 USA.
RP Berta, S (reprint author), Max Planck Inst Extraterr Phys MPE, Postfach 1312, D-85741 Garching, Germany.
EM berta@mpe.mpg.de
OI Gruppioni, Carlotta/0000-0002-5836-4056; Pozzetti,
Lucia/0000-0001-7085-0412; Santini, Paola/0000-0002-9334-8705;
Rodighiero, Giulia/0000-0002-9415-2296; Scott,
Douglas/0000-0002-6878-9840
FU BMVIT (Austria); ESA-PRODEX (Belgium); CEA/CNES (France); DLR (Germany);
ASI/INAF (Italy); CICYT/MCYT (Spain); CSA (Canada); NAOC (PR China);
CEA; CNES; CNRS (France); ASI (Italy); MCINN (Spain); SNSB (Sweden);
STFC; UKSA (UK); NASA (USA)
FX The authors wish to thank Dr. Jacopo Fritz for providing his library of
AGN torus emission models, and the anonymous referee for her/his useful
comments. This work made use of the code FASTEM, distributed by the
Auton Lab, and developed by Andrew Moore, Paul Hsiung, Peter Sand, point
of contact Saswati Ray. PACS has been developed by a consortium of
institutes led by MPE (Germany) and including UVIE (Austria); KU Leuven,
CSL, IMEC (Belgium); CEA, LAM(France); MPIA (Germany);
INAF-IFSI/OAA/OAP/OAT, LENS, SISSA (Italy); IAC (Spain). This
development has been supported by the funding agencies BMVIT (Austria),
ESA-PRODEX (Belgium), CEA/CNES (France), DLR (Germany), ASI/INAF
(Italy), and CICYT/MCYT (Spain). SPIRE has been developed by a
consortium of institutes led by Cardiff University (UK) and including
University of Lethbridge (Canada), NAOC (PR China), CEA, LAM (France),
IFSI, University of Padua (Italy), IAC (Spain), Stockholm Observatory
(Sweden), Imperial College London, RAL, UCL-MSSL, UKATC, University of
Sussex (UK), Caltech, JPL, NHSC, University of Colorado (USA). This
development has been supported by national funding agencies: CSA
(Canada); NAOC (PR China); CEA, CNES, CNRS (France); ASI (Italy); MCINN
(Spain); SNSB (Sweden); STFC, UKSA (UK) and NASA (USA).
NR 116
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PI LES ULIS CEDEX A
PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A,
FRANCE
SN 0004-6361
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD MAR
PY 2013
VL 551
AR A100
DI 10.1051/0004-6361/201220859
PG 22
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 110QR
UT WOS:000316460600100
ER
PT J
AU D'Elia, V
Perri, M
Puccetti, S
Capalbi, M
Giommi, P
Burrows, DN
Campana, S
Tagliaferri, G
Cusumano, G
Evans, P
Gehrels, N
Kennea, J
Moretti, A
Nousek, JA
Osborne, JP
Romano, P
Stratta, G
AF D'Elia, V.
Perri, M.
Puccetti, S.
Capalbi, M.
Giommi, P.
Burrows, D. N.
Campana, S.
Tagliaferri, G.
Cusumano, G.
Evans, P.
Gehrels, N.
Kennea, J.
Moretti, A.
Nousek, J. A.
Osborne, J. P.
Romano, P.
Stratta, G.
TI The seven year Swift-XRT point source catalog (1SWXRT)
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE catalogs; surveys; X-rays: general
ID X-RAY TELESCOPE; XMM-NEWTON; BLAZARS; CHANDRA
AB Context. The Swift satellite is a multi-wavelength observatory specifically designed for gamma-ray burst (GRB) astronomy that is operational since 2004. Swift is also a very flexible multi-purpose facility that supports a wide range of scientific fields such as active galactic nuclei, supernovae, cataclysmic variables, Galactic transients, active stars and comets. The Swift X-ray Telescope (XRT) has collected more than 150 Ms of observations in its first seven years of operations.
Aims. The purpose of this work is to present to the scientific community the list of all the X-ray point sources detected in XRT imaging data taken in photon counting mode during the first seven years of Swift operations. All these point-like sources, excluding the GRB, will be stored in a catalog publicly available (1SWXRT).
Methods. We considered all the XRT observations with exposure time longer than 500 s taken in the period 2005-2011. Data were reduced and analyzed with standard techniques and a list of detected sources for each observation was produced. A careful visual inspection was performed to remove extended, spurious and piled-up sources. Finally, positions, count rates, fluxes, and the corresponding uncertainties were computed.
Results. We have analyzed more than 35 000 XRT fields, with exposures ranging between 500 s and 100 ks, for a total exposure time of almost 140 Ms. The catalog includes approximately 89 000 entries, of which almost 85 000 are not affected by pile-up and are not GRBs. Considering that many XRT fields were observed several times, we have a total of similar to 36 000 distinct celestial sources. We computed count rates in three energy bands: 0.3-10 keV (Full, or F), 0.3-3 keV (Soft, or S) and 2-10 keV (Hard, or H). Each entry has a detection in at least one of these bands. In particular, we detect similar to 80 000, similar to 70 000 and similar to 25 500 in the F, S and H band, respectively. Count rates were converted into fluxes in the 0.5-10, 0.5-2 and 2-10 keV bands. The flux interval sampled by the detected sources is 7.4x10(-15)-9.1x10(-11), 3.1x10(-15)-1.1x10(-11) and 1.3x10(-14)-9.1x10(-11) erg cm(-2) s(-1) for the F, S and H band, respectively. Some possible scientific uses of the catalog are also highlighted.
C1 [D'Elia, V.; Perri, M.; Puccetti, S.; Capalbi, M.; Giommi, P.; Stratta, G.] ASI Sci Data Ctr, I-00044 Frascati, Italy.
[D'Elia, V.; Perri, M.; Puccetti, S.; Capalbi, M.; Stratta, G.] INAF Osservatorio Astron Roma, I-00040 Monte Porzio Catone, Italy.
[Burrows, D. N.; Kennea, J.; Nousek, J. A.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA.
[Campana, S.; Tagliaferri, G.; Moretti, A.] INAF Osservatorio Astron Brera, I-23807 Merate, LC, Italy.
[Cusumano, G.; Romano, P.] INAF Ist Astrofis Spaziale & Fis Cosm Palermo, I-90146 Palermo, Italy.
[Evans, P.; Osborne, J. P.] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England.
[Gehrels, N.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP D'Elia, V (reprint author), ASI Sci Data Ctr, Via Galileo Galilei, I-00044 Frascati, Italy.
EM delia@mporzio.astro.it
RI Stratta, Maria Giuliana/L-3045-2016;
OI Stratta, Maria Giuliana/0000-0003-1055-7980; Campana,
Sergio/0000-0001-6278-1576; giommi, paolo/0000-0002-2265-5003; D'Elia,
Valerio/0000-0002-7320-5862; Cusumano, Giancarlo/0000-0002-8151-1990;
Perri, Matteo/0000-0003-3613-4409; moretti, alberto/0000-0002-9770-0315;
Puccetti, Simonetta/0000-0002-2734-7835; Tagliaferri,
Gianpiero/0000-0003-0121-0723
FU ASI [I/004/11/0]; UK Space Agency
FX We thank the referee for a quick and careful reading of the manuscript.
This work has been supported by ASI grant I/004/11/0. J.P.O.
acknowledges financial support from the UK Space Agency.
NR 25
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PI LES ULIS CEDEX A
PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A,
FRANCE
SN 0004-6361
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD MAR
PY 2013
VL 551
AR A142
DI 10.1051/0004-6361/201220863
PG 11
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 110QR
UT WOS:000316460600142
ER
PT J
AU Feuchtgruber, H
Lellouch, E
Orton, G
de Graauw, T
Vandenbussche, B
Swinyard, B
Moreno, R
Jarchow, C
Billebaud, F
Cavalie, T
Sidher, S
Hartogh, P
AF Feuchtgruber, H.
Lellouch, E.
Orton, G.
de Graauw, T.
Vandenbussche, B.
Swinyard, B.
Moreno, R.
Jarchow, C.
Billebaud, F.
Cavalie, T.
Sidher, S.
Hartogh, P.
TI The D/H ratio in the atmospheres of Uranus and Neptune from
Herschel-PACS observations
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE planets and satellites: interiors; planets and satellites: individual:
Uranus; planets and satellites: atmospheres; planets and satellites:
individual: Neptune
ID ROTOTRANSLATIONAL ABSORPTION-SPECTRA; INFRARED ROTATIONAL SPECTRUM;
ISO-SWS OBSERVATIONS; OUTER SOLAR-SYSTEM; GIANT PLANETS;
CARBON-MONOXIDE; COLLISIONAL INTERFERENCE; WAVELENGTH SPECTROMETER;
MONODEUTERATED METHANE; HD
AB Herschel-PACS measurements of the rotational R(0) and R(1) HD lines in the atmospheres of Uranus and Neptune are analyzed to derive a D/H ratio with improved precision for the two planets. The derivation of the D/H ratio also includes previous measurements of the R(2) line with the Short Wavelength Spectrometer on board the Infrared Space Observatory (ISO). The available spectroscopic line information of the three rotational transitions is discussed and applied in the radiative transfer calculations. The best simultaneous fit of all three lines requires only a minor departure from the Spitzer temperature profile of Uranus and a departure limited to 2K from the Voyager temperature profile of Neptune (each time around the tropopause). The resulting and remarkably similar D/H ratios for Uranus and Neptune are found to be (4.4 +/- 0.4) x 10(-5) and (4.1 +/- 0.4) x 10(-5), respectively. Although the deuterium enrichment in the two atmospheres compared to the protosolar value is confirmed, it is found to be lower compared to previous analyses. Using interior models from the literature and assuming that complete mixing of the atmosphere and interior occured during the planets' history, we derive a D/H in protoplanetary ices between (5.75-7.0) x 10(-5) for Uranus and between (5.1-7.7) x 10(-5) for Neptune. Conversely, adopting a cometary D/H for the protoplanetary ices between (15-30) x 10(-5), we constrain the interior models of the two planets to have an ice mass fraction of 14-32%, i.e., the two planets are rock-dominated.
C1 [Feuchtgruber, H.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany.
[Lellouch, E.; Moreno, R.] Observ Paris, LESIA, F-92195 Meudon, France.
[Orton, G.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[de Graauw, T.] ALMA Observ, Santiago, Chile.
[Vandenbussche, B.] Katholieke Univ Leuven, Inst Sterrenkunde, B-3001 Louvain, Belgium.
[Swinyard, B.; Sidher, S.] Rutherford Appleton Lab, Didcot, Oxon, England.
[Swinyard, B.] UCL, London WC1E 6BT, England.
[Jarchow, C.; Hartogh, P.] Max Planck Inst Solar Syst Res, D-37191 Katlenburg Lindau, Germany.
[Billebaud, F.; Cavalie, T.] Univ Bordeaux, LAB, UMR 5804, F-33270 Floirac, France.
[Billebaud, F.; Cavalie, T.] CNRS, LAB, UMR 5804, F-33270 Floirac, France.
RP Feuchtgruber, H (reprint author), Max Planck Inst Extraterr Phys, Giessenbachstr, D-85748 Garching, Germany.
EM fgb@mpe.mpg.de
FU Centre National d'Etudes Spatiales (CNES); Programme National de
Plantologie (PNP) of CNRS/INSU
FX We thank Bruno Bezard for important advice on the HD line parameters,
and Dominique Bockelee-Morvan for discussions on the D/H ratio in
meteorites and comets. G. Orton carried out a part of this research at
the Jet Propulsion Laboratory, California Institute of Technology, under
a constract with NASA. T. Cavalie wishes to thank the Centre National
d'Etudes Spatiales (CNES) for funding. F. Billebaud acknowledges
multi-annual funding from the Programme National de Plantologie (PNP) of
CNRS/INSU. PACS has been developed by a consortium of institutes led by
MPE (Germany) and including UVIE (Austria); KUL, CSL, IMEC (Belgium);
CEA, OAMP (France); MPIA (Germany); IFSI, OAP /AOT, OAA /CAISMI, LENS,
SISSA (Italy); IAC (Spain). This development has been supported by the
funding agencies BMVIT (Austria), ESA-PRODEX (Belgium), CEA /CNES
(France), DLR (Germany), ASI (Italy), and CICYT /MCYT (Spain).
NR 66
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U1 2
U2 21
PU EDP SCIENCES S A
PI LES ULIS CEDEX A
PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A,
FRANCE
SN 0004-6361
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD MAR
PY 2013
VL 551
AR A126
DI 10.1051/0004-6361/201220857
PG 9
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 110QR
UT WOS:000316460600126
ER
PT J
AU Kospal, A
Abraham, P
Acosta-Pulido, JA
Morales, MJA
Balog, Z
Carnerero, MI
Szegedi-Elek, E
Farkas, A
Henning, T
Kelemen, J
Kovacs, T
Kun, M
Marton, G
Meszaros, S
Moor, A
Pal, A
Sarneczky, K
Szakats, R
Szalai, N
Szing, A
Toth, I
Turner, NJ
Vida, K
AF Kospal, A.
Abraham, P.
Acosta-Pulido, J. A.
Arevalo Morales, M. J.
Balog, Z.
Carnerero, M. I.
Szegedi-Elek, E.
Farkas, A.
Henning, Th
Kelemen, J.
Kovacs, T.
Kun, M.
Marton, G.
Meszaros, Sz
Moor, A.
Pal, A.
Sarneczky, K.
Szakats, R.
Szalai, N.
Szing, A.
Toth, I.
Turner, N. J.
Vida, K.
TI Exploring the circumstellar environment of the young eruptive star V2492
Cygni
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE stars: formation; circumstellar matter; infrared: stars; stars:
individual: V2492 Cyg
ID OUTBURST; EXTINCTION; NEBULA; PERFORMANCE; PHOTOMETRY; ACCRETION;
MISSION; MINIMA; LIGHT; DISKS
AB Context. V2492 Cyg is a young eruptive star that went into outburst in 2010. The near-infrared color changes observed since the outburst peak suggest that the source belongs to a newly defined sub-class of young eruptive stars, where time-dependent accretion and variable line-of-sight extinction play a combined role in the flux changes.
Aims. In order to learn about the origin of the light variations and to explore the circumstellar and interstellar environment of V2492 Cyg, we monitored the source at ten different wavelengths, between 0.55 mu m and 2.2 mu m from the ground and between 3.6 mu m and 160 mu m from space.
Methods. We analyze the light curves and study the color-color diagrams via comparison with the standard reddening path. We examine the structure of the molecular cloud hosting V2492 Cyg by computing temperature and optical depth maps from the far-infrared data.
Results. We find that the shapes of the light curves at different wavelengths are strictly self-similar and that the observed variability is related to a single physical process, most likely variable extinction. We suggest that the central source is episodically occulted by a dense dust cloud in the inner disk and, based on the invariability of the far-infrared fluxes, we propose that it is a long-lived rather than a transient structure. In some respects, V2492 Cyg can be regarded as a young, embedded analog of UX Orionis-type stars.
Conclusions. The example of V2492 Cyg demonstrates that the light variations of young eruptive stars are not exclusively related to changing accretion. The variability provided information on an azimuthally asymmetric structural element in the inner disk. Such an asymmetric density distribution in the terrestrial zone may also have consequences for the initial conditions of planet formation.
C1 [Kospal, A.] European Space Agcy, Estec, SRE SA, Res & Sci Support Dept, NL-2200 AG Noordwijk, Netherlands.
[Abraham, P.; Szegedi-Elek, E.; Farkas, A.; Kelemen, J.; Kovacs, T.; Kun, M.; Marton, G.; Moor, A.; Pal, A.; Sarneczky, K.; Szakats, R.; Szalai, N.; Szing, A.; Toth, I.; Vida, K.] Hungarian Acad Sci, Res Ctr Astron & Earth Sci, Konkoly Observ, H-1525 Budapest, Hungary.
[Acosta-Pulido, J. A.; Arevalo Morales, M. J.; Carnerero, M. I.; Meszaros, Sz] Inst Astrofis Canarias, Tenerife 38200, Spain.
[Acosta-Pulido, J. A.; Arevalo Morales, M. J.; Carnerero, M. I.; Meszaros, Sz] Univ La Laguna, Dept Astrofis, Tenerife 38205, Spain.
[Balog, Z.; Henning, Th] Max Planck Inst Astron, D-69117 Heidelberg, Germany.
[Pal, A.] Eotvos Lorand Univ, Dept Astron, H-1117 Budapest, Hungary.
[Sarneczky, K.] ELTE Gothard Lendulet Res Grp, H-9700 Szombathely, Hungary.
[Turner, N. J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Kospal, A (reprint author), European Space Agcy, Estec, SRE SA, Res & Sci Support Dept, POB 299, NL-2200 AG Noordwijk, Netherlands.
EM akospal@rssd.esa.int
RI Meszaros, Szabolcs/N-2287-2014
OI Meszaros, Szabolcs/0000-0001-8237-5209
FU Hungarian Scientific Research Fund [OTKA-101393, OTKA-104607, OTKA
K-81373, OTKA K-81966]; Hungarian Academy of Sciences; MAG Zrt [HUMAN
MB08C 81013]; Janos Bolyai Research Scholarship of Hungarian Academy of
Sciences; [LP2012-31/2012]
FX We thank the referee, Dr. V. Grinin, for his valuable comments, in
particular those emphasizing the physical similarity between V2492 Cyg
and the UX Orionis-type stars. We acknowledge with thanks the variable
star observations from the AAVSO International Database contributed by
observers worldwide and used in this research, including recent
monitoring by James Roe obtained through the Lowell Amateur Research
Initiative. This work was partly supported by the grants OTKA-101393,
OTKA-104607, OTKA K-81373, and OTKA K-81966 of the Hungarian Scientific
Research Fund, by the Lendulet-2009 Young Researchers' Program of the
Hungarian Academy of Sciences, by the HUMAN MB08C 81013 grant of the MAG
Zrt, by the Janos Bolyai Research Scholarship of the Hungarian Academy
of Sciences, and by the grant LP2012-31/2012. The William Herschel
Telescope and its service program are operated on the island of La Palma
by the Isaac Newton Group in the Spanish Observatorio del Roque de los
Muchachos of the Instituto de Astrofisica de Canarias. This work is
based in part on observations made with the Telescopio Carlos Sanchez
operated on the island of Tenerife by the Instituto de Astrofisica de
Canarias in the Observatorio del Teide. The authors wish to thank the
telescope manager A. Oscoz, the support astronomers and telescope
operators for their help during the observations, as well as the service
mode observers. PACS has been developed by a consortium of institutes
led by MPE (Germany) and including UVIE (Austria); KUL, CSL, IMEC
(Belgium); CEA, OAMP (France); MPIA (Germany); IFSI, OAP/AOT,
OAA/CAISMI, LENS, SISSA (Italy); IAC (Spain). This development has been
supported by the funding agencies BMVIT (Austria), ESA-PRODEX (Belgium),
CEA/CNES (France), DLR (Germany), ASI (Italy), and CICT/MCT (Spain).
SPIRE has been developed by a consortium of institutes led by Cardiff
Univ. (UK) and including Univ. Lethbridge (Canada); NAOC (China); CEA,
LAM (France); IFSI, Univ. Padua (Italy); IAC (Spain); Stockholm
Observatory (Sweden); Imperial College London, RAL, UCL-MSSL, UKATC,
Univ. Sussex (UK); and Caltech, JPL, NHSC, Univ. Colorado (USA). This
development has been supported by national funding agencies: CSA
(Canada); NAOC (China); CEA, CNES, CNRS (France); ASI (Italy); MCINN
(Spain); SNSB (Sweden); STFC (UK); and NASA (USA).
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SN 0004-6361
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD MAR
PY 2013
VL 551
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SC Astronomy & Astrophysics
GA 110QR
UT WOS:000316460600062
ER
PT J
AU Lippi, M
Villanueva, GL
DiSanti, MA
Bohnhardt, H
Mumma, MJ
Bonev, BP
Prialnik, D
AF Lippi, M.
Villanueva, G. L.
DiSanti, M. A.
Boehnhardt, H.
Mumma, M. J.
Bonev, B. P.
Prialnik, D.
TI A new model for the nu(1) vibrational band of HCN in cometary comae,
with application to three comets
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE molecular data; astrobiology; comets: individual: 8P/Tuttle; comets:
individual: C/2007W1 (Boattini); infrared: general; comets: individual:
C/2008 Q3 (Garradd)
ID O1 HALE-BOPP; ROTATIONAL TEMPERATURE; INFRARED OBSERVATIONS; VOLATILE
COMPOSITION; WATER; 8P/TUTTLE; (HCN)-C-12-N-14; IDENTIFICATION;
COEFFICIENTS; TRANSITIONS
AB Aims. Hydrogen cyanide (HCN) radiates effectively at infrared wavelengths in cometary atmospheres, and a new quantum-band model is needed to properly interpret high-resolution spectra. HCN spectra of comets 8P/Tuttle, C/2007 W1 (Boattini), and C/2008 Q3 (Garradd) have been recorded by our team using the high-resolution CRyogenic InfraRed Echelle Spectometer (CRIRES) at the Very Large Telescope (VLT), ultimately posing an excellent test for our newly developed model.
Methods. We developed a quantum-band model for the nu(1) fundamental of HCN using the latest spectroscopic parameters available and with it retrieved HCN in the above mentioned three comets. For each comet, we sampled several lines of HCN in the spectral region near 3 mu m, and retrieved molecular production rates, mixing ratios, and rotational temperatures.
Results. When compared to other comets, 8P/Tuttle is relatively depleted in HCN, while C/2007 W1 (Boattini) appears to be enriched and C/2008 Q3 (Garradd) normal. The spatial profile of HCN observed in 8P/Tuttle is symmetric, consistent with isotropic outgassing from the nucleus, while in comet C/2007 W1 we observed an asymmetric excess of HCN in the anti-solar direction. We investigated the HCN-CN parentage by comparing our production rate ratios (HCN/H2O) with those of CN/OH derived at optical wavelengths. In comet C/2007 W1 the two mixing ratios are comparable, while in 8P/Tuttle our derived HCN abundance is too low to support the HCN molecule as the only parent of the CN radical.
C1 [Lippi, M.; Boehnhardt, H.] Max Planck Inst Solar Syst Res, Katlenburg Lindau, Germany.
[Villanueva, G. L.; DiSanti, M. A.; Mumma, M. J.; Bonev, B. P.] NASA, Goddard Space Flight Ctr, Goddard Ctr Astrobiol, Greenbelt, MD 20771 USA.
[Prialnik, D.] Tel Aviv Univ, Dept Geophys & Planetary Sci, IL-69978 Tel Aviv, Israel.
[Bonev, B. P.] Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA.
RP Lippi, M (reprint author), Max Planck Inst Solar Syst Res, Katlenburg Lindau, Germany.
EM ciortellina@gmail.com
RI mumma, michael/I-2764-2013
FU International Max Planck Research School; NASA's Planetary Astronomy
Program, Astrobiology Program and Postdoctoral Program; German-Israeli
Foundation for Scientific Research and Development
FX We thank the VLT science operations team of the European Southern
Observatory for efficient execution of the observations. This work was
supported by the International Max Planck Research School, NASA's
Planetary Astronomy Program, Astrobiology Program and Postdoctoral
Program and the German-Israeli Foundation for Scientific Research and
Development.
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SN 1432-0746
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD MAR
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GA 110QR
UT WOS:000316460600051
ER
PT J
AU Muller, S
Ferrigno, C
Kuhnel, M
Schonherr, G
Becker, PA
Wolff, MT
Hertel, D
Schwarm, FW
Grinberg, V
Obst, M
Caballero, I
Pottschmidt, K
Furst, F
Kreykenbohm, I
Rothschild, RE
Hemphill, P
Nunez, SM
Torrejon, JM
Klochkov, D
Staubert, R
Wilms, J
AF Mueller, S.
Ferrigno, C.
Kuehnel, M.
Schoenherr, G.
Becker, P. A.
Wolff, M. T.
Hertel, D.
Schwarm, F. -W.
Grinberg, V.
Obst, M.
Caballero, I.
Pottschmidt, K.
Fuerst, F.
Kreykenbohm, I.
Rothschild, R. E.
Hemphill, P.
Nunez, S. M.
Torrejon, J. M.
Klochkov, D.
Staubert, R.
Wilms, J.
TI No anticorrelation between cyclotron line energy and X-ray flux in 4U
0115+634
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE X-rays: binaries; pulsars: individual 4U 0115+634; magnetic fields
ID TIMING-EXPLORER; GIANT OUTBURST; RESONANCE ENERGIES; ABSORPTION FEATURE;
PULSAR 4U-0115+63; MAGNETIC-FIELDS; HIGH-RESOLUTION; NEUTRON-STARS;
INTEGRAL DATA; EXO 2030+375
AB We report on an outburst of the high mass X-ray binary 4U 0115+634 with a pulse period of 3.6 s in 2008 March/April as observed with RXTE and INTEGRAL. During the outburst the neutron star's luminosity varied by a factor of 10 in the 3-50 keV band. In agreement with earlier work we find evidence of five cyclotron resonance scattering features at similar to 10.7, 21.8, 35.5, 46.7, and 59.7 keV. Previous work had found an anticorrelation between the fundamental cyclotron line energy and the X-ray flux. We show that this apparent anticorrelation is probably due to the unphysical interplay of parameters of the cyclotron line with the continuum models used previously, e. g., the negative and positive exponent power law (NPEX). For this model, we show that cyclotron line modeling erroneously leads to describing part of the exponential cutoff and the continuum variability, and not the cyclotron lines. When the X-ray continuum is modeled with a simple exponentially cutoff power law modified by a Gaussian emission feature around 10 keV, the correlation between the line energy and the flux vanishes, and the line parameters remain virtually constant over the outburst. We therefore conclude that the previously reported anticorrelation is an artifact of the assumptions adopted in the modeling of the continuum.
C1 [Mueller, S.; Kuehnel, M.; Hertel, D.; Schwarm, F. -W.; Grinberg, V.; Obst, M.; Kreykenbohm, I.; Wilms, J.] Univ Erlangen Nurnberg, Dr Karl Remeis Observ, D-96049 Bamberg, Germany.
[Mueller, S.; Kuehnel, M.; Hertel, D.; Schwarm, F. -W.; Grinberg, V.; Obst, M.; Kreykenbohm, I.; Wilms, J.] Univ Erlangen Nurnberg, ECAP, D-96049 Bamberg, Germany.
[Ferrigno, C.] Univ Geneva, ISDC Data Ctr Astrophys, CH-1290 Versoix, Switzerland.
[Schoenherr, G.] Leibniz Inst Astrophys Potsdam, D-14482 Potsdam, Germany.
[Becker, P. A.] George Mason Univ, Sch Phys Astron & Computat Sci, Fairfax, VA 22030 USA.
[Wolff, M. T.] USN, Res Lab, Div Space Sci, Washington, DC 20375 USA.
[Caballero, I.] Univ Paris 07, CEA Saclay, CNRS, DSM IRFU SAp UMR AIM 7158,CEA, F-91191 Gif Sur Yvette, France.
[Pottschmidt, K.] CRESST, Greenbelt, MD 20771 USA.
[Pottschmidt, K.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Pottschmidt, K.] UMBC, Ctr Space Sci & Technol, Baltimore, MD 21250 USA.
[Fuerst, F.] CALTECH, Space Radiat Lab, Pasadena, CA 91125 USA.
[Rothschild, R. E.; Hemphill, P.] Univ Calif San Diego, Ctr Astrophys & Space Sci, La Jolla, CA 92093 USA.
[Nunez, S. M.; Torrejon, J. M.] Univ Alicante, Inst Univ Fis Aplicada Ciencias & Tecnol, E-03080 Alicante, Spain.
[Klochkov, D.; Staubert, R.] Univ Tubingen, Inst Astron & Astrophys, D-72076 Tubingen, Germany.
RP Muller, S (reprint author), Univ Erlangen Nurnberg, Dr Karl Remeis Observ, Sternwartstr 7, D-96049 Bamberg, Germany.
EM Sebastian.Mueller@sternwarte.uni-erlangen.de
RI Wilms, Joern/C-8116-2013; Kreykenbohm, Ingo/H-9659-2013; Torrejon, Jose
/K-6395-2014;
OI Wilms, Joern/0000-0003-2065-5410; Kreykenbohm, Ingo/0000-0001-7335-1803;
Torrejon, Jose /0000-0002-5967-5163; Hemphill, Paul/0000-0002-1676-6954
FU Bundesministerium fur Wirtschaft und Technologie under Deutsches Zentrum
fur Luft- und Raumfahrt [50OR0808, 50OR0905, 50OR1113]; Deutscher
Akademischer Austauschdienst; US Office of Naval Research; French Space
Agency CNES through CNRS; Spanish Ministerio de Ciencia, Tecnologia e
Innovacion (MCINN) [AYA2010-15431]; ESA; [AIB2010DE-00057]
FX We thank the referee for his/her insightful comments. We also thank the
schedulers of RXTE and INTEGRAL for their role in making this campaign
possible, and the International Space Science Institute in Bern,
Switzerland, for their hospitality. We acknowledge funding by the
Bundesministerium fur Wirtschaft und Technologie under Deutsches Zentrum
fur Luft- und Raumfahrt grants 50OR0808, 50OR0905, and 50OR1113, and by
the Deutscher Akademischer Austauschdienst. M. T. W. is supported by the
US Office of Naval Research. IC acknowledges financial support from the
French Space Agency CNES through CNRS. S.M.N. and J.M.T. acknowledge
support from the Spanish Ministerio de Ciencia, Tecnologia e Innovacion
(MCINN) through grant AYA2010-15431 and the use of the computer
facilities made available through the grant AIB2010DE-00057. This
research is in part based on observations with INTEGRAL, an ESA project
with instruments and science data centre funded by ESA member states
(especially the PI countries: Denmark, France, Germany, Italy,
Switzerland, Spain), Czech Republic, and Poland, and with the
participation of Russia and USA. We thank John E. Davis for the
development of the SLxfig module, which was used to create all figures
in the paper.
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J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD MAR
PY 2013
VL 551
AR A6
DI 10.1051/0004-6361/201220359
PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 110QR
UT WOS:000316460600006
ER
PT J
AU Omont, A
Yang, C
Cox, P
Neri, R
Beelen, A
Bussmann, RS
Gavazzi, R
van der Werf, P
Riechers, D
Downes, D
Krips, M
Dye, S
Ivison, R
Vieira, JD
Weiss, A
Aguirre, JE
Baes, M
Baker, AJ
Bertoldi, F
Cooray, A
Dannerbauer, H
De Zotti, G
Eales, SA
Fu, H
Gao, Y
Guelin, M
Harris, AI
Jarvis, M
Lehnert, M
Leeuw, L
Lupu, R
Menten, K
Michalowski, MJ
Negrello, M
Serjeant, S
Temi, P
Auld, R
Dariush, A
Dunne, L
Fritz, J
Hopwood, R
Hoyos, C
Ibar, E
Maddox, S
Smith, MWL
Valiante, E
Bock, J
Bradford, CM
Glenn, J
Scott, KS
AF Omont, A.
Yang, C.
Cox, P.
Neri, R.
Beelen, A.
Bussmann, R. S.
Gavazzi, R.
van der Werf, P.
Riechers, D.
Downes, D.
Krips, M.
Dye, S.
Ivison, R.
Vieira, J. D.
Weiss, A.
Aguirre, J. E.
Baes, M.
Baker, A. J.
Bertoldi, F.
Cooray, A.
Dannerbauer, H.
De Zotti, G.
Eales, S. A.
Fu, H.
Gao, Y.
Guelin, M.
Harris, A. I.
Jarvis, M.
Lehnert, M.
Leeuw, L.
Lupu, R.
Menten, K.
Michalowski, M. J.
Negrello, M.
Serjeant, S.
Temi, P.
Auld, R.
Dariush, A.
Dunne, L.
Fritz, J.
Hopwood, R.
Hoyos, C.
Ibar, E.
Maddox, S.
Smith, M. W. L.
Valiante, E.
Bock, J.
Bradford, C. M.
Glenn, J.
Scott, K. S.
TI H2O emission in high-z ultra-luminous infrared galaxies
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE galaxies: high-redshift; galaxies: starburst; infrared: galaxies;
submillimeter: galaxies; radio lines: galaxies
ID QUASAR APM 08279+5255; WATER-VAPOR EMISSION; DENSE MOLECULAR GAS;
STAR-FORMATION RATE; HERSCHEL-ATLAS; SUBMILLIMETER GALAXY;
HIGH-REDSHIFT; CLOVERLEAF QUASAR; IRAS 10214+4724; MARKARIAN 231
AB Using the IRAM Plateau de Bure interferometer (PdBI), we report the detection of water vapor in six new lensed ultra-luminous starburst galaxies at high redshift, discovered in the Herschel Astrophysical Terahertz Large Area Survey (H-ATLAS). The sources are detected either in the 2(02)-1(11) or 2(11)-2(02) H2O emission lines with integrated line fluxes ranging from 1.8 to 14 Jy km s(-1). The corresponding apparent luminosities are mu L-H2O similar to 3-12 x 10(8) L-circle dot, where mu is the lensing magnification factor (3 < mu < 12). These results confirm that H2O lines are among the strongest molecular lines in high-z ultra-luminous starburst galaxies, with intensities almost comparable to those of the high-J CO lines, and similar profiles and line widths (similar to 200-900 km s(-1)). With the current sensitivity of the PdBI, the water lines can therefore easily be detected in high-z lensed galaxies (with F(500 mu m) > 100 mJy) discovered in the Herschel surveys. Correcting the luminosities for amplification, using existing lensing models, L-H2O is found to have a strong dependence on the infrared luminosity, varying as similar to L-IR(1.2). This relation, which needs to be confirmed with better statistics, may indicate a role of radiative (infrared) excitation of the H2O lines, and implies that high-z galaxies with L-IR greater than or similar to 10(13) L-circle dot tend to be very strong emitters in water vapor, that have no equivalent in the local universe.
C1 [Omont, A.; Yang, C.; Gavazzi, R.] Univ Paris 06, Inst Astrophys Paris, UMR7095, F-75014 Paris, France.
[Omont, A.; Yang, C.; Gavazzi, R.] CNRS, Inst Astrophys Paris, UMR7095, F-75014 Paris, France.
[Yang, C.; Gao, Y.] Purple Mt Observ, Nanjing, Jiangsu, Peoples R China.
[Yang, C.] Beijing Normal Univ, Dept Astron, Beijing, Peoples R China.
[Cox, P.; Neri, R.; Downes, D.; Krips, M.; Guelin, M.] Inst Radio Astron Millimetr, F-38406 St Martin Dheres, France.
[Beelen, A.] Univ Paris 11, F-91405 Orsay, France.
[Beelen, A.] CNRS, Inst Astrophys Spatiale, UMR8617, F-91405 Orsay, France.
[Bussmann, R. S.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[van der Werf, P.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands.
[Riechers, D.] Cornell Univ, Dept Astron, Ithaca, NY 14853 USA.
[Dye, S.] Ctr Astron & Particle Theory, Nottingham NG7 2RD, England.
[Ivison, R.; Michalowski, M. J.] Univ Edinburgh, Royal Observ, Inst Astron, Edinburgh EH9 3HJ, Midlothian, Scotland.
[Aguirre, J. E.; Lupu, R.; Scott, K. S.] Univ Penn, Dept Phys & Astron, Philadelphia, PA 19104 USA.
[Baes, M.; Michalowski, M. J.; Fritz, J.] Univ Ghent, Sterrenkundig Observatorium, B-9000 Ghent, Belgium.
[Baker, A. J.] Rutgers State Univ, Dept Phys & Astron, Piscataway, NJ 08854 USA.
[Bertoldi, F.] Univ Bonn, Argelander Inst Astron, D-53121 Bonn, Germany.
[Dannerbauer, H.] Univ Vienna, Inst Astron, A-1180 Vienna, Austria.
[Eales, S. A.; Auld, R.; Dariush, A.; Smith, M. W. L.; Valiante, E.] Cardiff Univ, Sch Phys & Astron, Cardiff CF24 3AA, S Glam, Wales.
[Fu, H.] Univ Calif Irvine, Dept Phys & Astron, Irvine, CA 92697 USA.
[Harris, A. I.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Menten, K.] Max Planck Inst Radioastron, D-53121 Bonn, Germany.
[De Zotti, G.; Negrello, M.] INAF Osservatorio Astron Padova, I-35122 Padua, Italy.
[De Zotti, G.; Negrello, M.] SISSA, I-34136 Trieste, Italy.
[Serjeant, S.] Open Univ, Dept Phys & Astron, Milton Keynes MK7 6AA, Bucks, England.
[Temi, P.] NASA, Astrophys Branch, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Jarvis, M.] Univ Oxford, Dept Phys, Oxford OX1 3RH, England.
[Dariush, A.] Inst Res Fundamental Sci IPM, Sch Astron, Tehran, Iran.
[Maddox, S.] Univ Canterbury, Dept Phys & Astron, Christchurch 8140, New Zealand.
[Dunne, L.; Hoyos, C.] Univ Nottingham, Sch Phys & Astron, Nottingham NG7 2RD, England.
[Bock, J.; Bradford, C. M.] CALTECH, Pasadena, CA 91125 USA.
[Bock, J.; Bradford, C. M.] Jet Prop Lab, Pasadena, CA 91109 USA.
[Glenn, J.] Univ Colorado, CASA, Boulder, CO 80303 USA.
[Lehnert, M.] Univ Paris Diderot, CNRS, Observ Paris, GEPI, F-92190 Meudon, France.
[Ibar, E.] Royal Observ, UK Astron Technol Ctr, Edinburgh EH9 3HJ, Midlothian, Scotland.
[Ibar, E.] Univ Catolica Chile, Dept Astron & Astrofis, Santiago 22, Chile.
[Jarvis, M.] Univ Western Cape, Dept Phys, ZA-7535 Bellville, South Africa.
[Hopwood, R.] Univ London Imperial Coll Sci Technol & Med, Blackett Lab, Astrophys Grp, London SW7 2AZ, England.
[Leeuw, L.] Univ S Africa, Coll Grad Studies, ZA-003 Unisa, South Africa.
RP Omont, A (reprint author), Univ Paris 06, Inst Astrophys Paris, UMR7095, F-75014 Paris, France.
EM omont@iap.fr
RI YANG, Chentao/H-1966-2015; Ivison, R./G-4450-2011; Baes,
Maarten/I-6985-2013; Lupu, Roxana/P-9060-2014
OI YANG, Chentao/0000-0002-8117-9991; Ivison, R./0000-0001-5118-1313; De
Zotti, Gianfranco/0000-0003-2868-2595; Maddox,
Stephen/0000-0001-5549-195X; De Hoyos Fernandez De Cordova,
Carlos/0000-0003-3120-6856; Dye, Simon/0000-0002-1318-8343; Baes,
Maarten/0000-0002-3930-2757; Lupu, Roxana/0000-0003-3444-5908
FU INSU/CNRS (France); MPG (Germany); IGN (Spain); NASA through JPL;
ASI-INAF [I/009/10/0]; CSA (Canada); NAOC (China); CEA; CNES; CNRS
(France); ASI (Italy); MCINN (Spain); SNSB (Sweden); STFC; UKSA (UK);
NASA (USA); FWO-Pegasus Marie Curie Fellowship
FX Based on observations carried out with the IRAM Plateau de Bure
interferometer. IRAM is supported by INSU/CNRS (France), MPG (Germany)
and IGN (Spain). The authors are grateful to the IRAM staff for their
support. US participants in H-ATLAS acknowledge support from NASA
through a contract from JPL. Italian participants in H-ATLAS acknowledge
a financial contribution from the agreement ASI-INAF I/009/10/0. SPIRE
has been developed by a consortium of institutes led by Cardiff Univ.
(UK) and including: Univ. Lethbridge (Canada); NAOC (China); CEA, LAM
(France); IFSI, Univ. Padua (Italy); IAC (Spain); Stockholm Observatory
(Sweden); Imperial College London, RAL, UCL-MSSL, UKATC, Univ. Sussex
(UK); and Caltech, JPL, NHSC, Univ. Colorado (USA). This development has
been supported by national funding agencies: CSA (Canada); NAOC (China);
CEA, CNES, CNRS (France); ASI (Italy); MCINN (Spain); SNSB (Sweden);
STFC, UKSA (UK); and NASA (USA). M.J. Michalowski acknowledges the
support of a FWO-Pegasus Marie Curie Fellowship.
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JI Astron. Astrophys.
PD MAR
PY 2013
VL 551
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DI 10.1051/0004-6361/201220811
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 110QR
UT WOS:000316460600115
ER
PT J
AU Ricci, D
Elyiv, A
Finet, F
Wertz, O
Alsubai, K
Anguita, T
Bozza, V
Browne, P
Burgdorf, M
Novati, SC
Dodds, P
Dominik, M
Dreizler, S
Gerner, T
Glitrup, M
Grundahl, F
Hardis, S
Harpsoe, K
Hinse, TC
Hornstrup, A
Hundertmark, M
Jorgensen, UG
Kains, N
Kerins, E
Liebig, C
Maier, G
Mancini, L
Masi, G
Mathiasen, M
Penny, M
Proft, S
Rahvar, S
Scarpetta, G
Sahu, K
Schafer, S
Schonebeck, F
Schmidt, R
Skottfelt, J
Snodgrass, C
Southworth, J
Thoene, CC
Wambsganss, J
Zimmer, F
Zub, M
Surdej, J
AF Ricci, D.
Elyiv, A.
Finet, F.
Wertz, O.
Alsubai, K.
Anguita, T.
Bozza, V.
Browne, P.
Burgdorf, M.
Novati, S. Calchi
Dodds, P.
Dominik, M.
Dreizler, S.
Gerner, T.
Glitrup, M.
Grundahl, F.
Hardis, S.
Harpsoe, K.
Hinse, T. C.
Hornstrup, A.
Hundertmark, M.
Jorgensen, U. G.
Kains, N.
Kerins, E.
Liebig, C.
Maier, G.
Mancini, L.
Masi, G.
Mathiasen, M.
Penny, M.
Proft, S.
Rahvar, S.
Scarpetta, G.
Sahu, K.
Schaefer, S.
Schoenebeck, F.
Schmidt, R.
Skottfelt, J.
Snodgrass, C.
Southworth, J.
Thoene, C. C.
Wambsganss, J.
Zimmer, F.
Zub, M.
Surdej, J.
TI Flux and color variations of the doubly imaged quasar UM673
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE gravitational lensing: strong; quasars: general; techniques:
photometric; quasars: individual: UM673
ID GRAVITATIONAL LENSES; TIME-DELAY; UM-673; VARIABILITY
AB Aims. With the aim of characterizing the flux and color variations of the multiple components of the gravitationally lensed quasar UM673 as a function of time, we have performed multiepoch and multiband photometric observations with the Danish 1.54 m telescope at the La Silla Observatory.
Methods. The observations were carried out in the VRi spectral bands during four seasons (2008-2011). We reduced the data using the point spread function photometric technique as well as aperture photometry.
Results. Our results show for the brightest lensed component some significant decrease in flux between the first two seasons (+0.09/+0.11/+0.05 mag) and a subsequent increase during the following ones (-0.11/-0.11/-0.10 mag) in the V/R/i spectral bands, respectively. Comparing our results with previous studies, we find smaller color variations between these seasons as compared with previous ones. We also separate the contribution of the lensing galaxy from that of the fainter and close lensed component.
C1 [Ricci, D.; Elyiv, A.; Finet, F.; Surdej, J.] Univ Liege, Dept Astrophys Geophys & Oceanog, B-4000 Liege 1, Belgium.
[Elyiv, A.] Ukrainian Acad Sci, Main Astron Observ, UA-03680 Kiev, Ukraine.
[Anguita, T.] Pontificia Univ Catolica Chile, Dept Astron & Astrofis, Ctr Astroingn, Santiago, Chile.
[Anguita, T.; Mancini, L.] Max Planck Inst Astron, D-69117 Heidelberg, Germany.
[Bozza, V.; Novati, S. Calchi; Mancini, L.; Scarpetta, G.] Univ Salerno, Dipartimento Fis ER Caianiello, I-84085 Fisciano, SA, Italy.
[Bozza, V.; Scarpetta, G.] Ist Nazl Fis Nucl, Sez Napoli, Naples, Italy.
[Browne, P.; Dodds, P.; Dominik, M.; Kains, N.; Liebig, C.] Univ St Andrews, SUPA, Sch Phys & Astron, St Andrews KY16 9SS, Fife, Scotland.
[Burgdorf, M.] Univ Stuttgart, Deutsch SOFIA Inst, D-70569 Stuttgart, Germany.
[Novati, S. Calchi] Ist Int Alti Studi Sci IIASS, Vietri Sul Mare, SA, Italy.
[Dreizler, S.; Hundertmark, M.; Schaefer, S.] Univ Gottingen, Inst Astrophys, D-37077 Gottingen, Germany.
[Glitrup, M.; Grundahl, F.] Aarhus Univ, Dept Phys & Astron, DK-8000 Aarhus C, Denmark.
[Hardis, S.; Harpsoe, K.; Hinse, T. C.; Jorgensen, U. G.; Mathiasen, M.; Skottfelt, J.] Univ Copenhagen, Niels Bohr Inst, DK-2100 Copenhagen O, Denmark.
[Hinse, T. C.] KASI Korea Astron & Space Sci Inst, Taejon 305348, South Korea.
[Hornstrup, A.] Tech Univ Denmark, Natl Space Inst, DK-2800 Lyngby, Denmark.
[Gerner, T.; Liebig, C.; Maier, G.; Proft, S.; Schoenebeck, F.; Schmidt, R.; Wambsganss, J.; Zimmer, F.; Zub, M.] Heidelberg Univ, Zentrum Astron, Astron Rechen Inst, D-69120 Heidelberg, Germany.
[Mancini, L.] Univ Sannio, Dipartimento Ingn, I-82100 Benevento, Italy.
[Masi, G.] Bellatrix Astron Observ, Ctr Backyard Astrophys, Ceccano, FR, Italy.
[Rahvar, S.] Sharif Univ Technol, Dept Phys, Tehran, Iran.
[Snodgrass, C.] European So Observ, Santiago 19, Chile.
[Snodgrass, C.] Max Planck Inst Solar Syst Res, D-37191 Katlenburg Lindau, Germany.
[Southworth, J.] Keele Univ, Astrophys Grp, Keele ST5 5BG, Staffs, England.
[Thoene, C. C.] Univ Copenhagen, Niels Bohr Inst, Dark Cosmol Ctr, DK-2100 Copenhagen, Denmark.
[Thoene, C. C.] INAF, Osservatorio Astron Brera, I-23807 Merate, Italy.
[Burgdorf, M.] NASA, SOFIA Sci Ctr, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Harpsoe, K.; Jorgensen, U. G.] Geol Museum, Ctr Star & Planet Format, DK-1350 Copenhagen, Denmark.
[Kerins, E.; Penny, M.] Univ Manchester, Jodrell Bank Ctr Astrophy, Manchester M13 9PL, Lancs, England.
[Rahvar, S.] Perimeter Inst Theoret Phys, Waterloo, ON N2L 2Y5, Canada.
[Ricci, D.] INAF Ist Astrofis Spaziale & Fis Cosm, I-40129 Bologna, Italy.
[Ricci, D.] Univ Nacl Autonoma Mexico, Inst Astron, Ensenada 22800, Baja California, Mexico.
[Anguita, T.] Univ Andres Bello, Dept Ciencias Fis, Santiago, Chile.
RP Ricci, D (reprint author), Univ Liege, Dept Astrophys Geophys & Oceanog, Bat B5C, B-4000 Liege 1, Belgium.
EM ricci@astro.ulg.ac.be
RI Zimmer, Fabian/M-4765-2014; Hundertmark, Markus/C-6190-2015; Rahvar,
Sohrab/A-9350-2008;
OI Hundertmark, Markus/0000-0003-0961-5231; Rahvar,
Sohrab/0000-0002-7084-5725; Dominik, Martin/0000-0002-3202-0343; Thone,
Christina/0000-0002-7978-7648; Ricci, Davide/0000-0002-9790-0552; Penny,
Matthew/0000-0001-7506-5640; Snodgrass, Colin/0000-0001-9328-2905
FU ARC - Action de recherche concertee (Communaute Francaise de Belgique -
Academie Wallonie-Europe); European Union [283783]; Belgian Federal
Science Policy Office; NASU Target Program "CosmoMicroPhysics"; European
Community [229517]; Qatar Foundation from QNRF [NPRP-09-476-1-078];
Danish National Science Research Council (FNU)
FX This research was supported by ARC - Action de recherche concertee
(Communaute Francaise de Belgique - Academie Wallonie-Europe). D.R.
(boursier FRIA) acknlowledges GLObal Robotic telescopes Intelligent
Array for e-Science (GLORIA), a project funded by the European Union
Seventh Framework Programme (FP7/2007-2012) under grant agreement number
283783. A.E. is the beneficiary of a fellowship granted by the Belgian
Federal Science Policy Office. A.E. is also grateful for partial support
in the framework of the NASU Target Program "CosmoMicroPhysics". N.K.
received funding from the European Community's Seventh Framework
Programme (/FP7/2007-2013/) under grant agreement No 229517. M.D., M.H.
and C.L. acknowledge the Qatar Foundation for support from QNRF grant
NPRP-09-476-1-078. Operation of the Danish 1.54 m telescope is supported
by the Danish National Science Research Council (FNU).
NR 23
TC 4
Z9 4
U1 0
U2 5
PU EDP SCIENCES S A
PI LES ULIS CEDEX A
PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A,
FRANCE
SN 0004-6361
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD MAR
PY 2013
VL 551
AR A104
DI 10.1051/0004-6361/201118755
PG 7
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 110QR
UT WOS:000316460600104
ER
PT J
AU Geissler, PE
Stantzos, NW
Bridges, NT
Bourke, MC
Silvestro, S
Fenton, LK
AF Geissler, Paul E.
Stantzos, Nicholas W.
Bridges, Nathan T.
Bourke, Mary C.
Silvestro, Simone
Fenton, Lori K.
TI Shifting sands on Mars: insights from tropical intra-crater dunes
SO EARTH SURFACE PROCESSES AND LANDFORMS
LA English
DT Article
DE Mars; dunes; saltation
AB Evidence for sand motion is found in repeated observations of sand dunes at three sites in the Martian tropics by the High Resolution Imaging Science Experiment on Mars Reconnaissance Orbiter. An eroding outcrop of layered sediments is identified as a possible source of the sand in Pasteur crater. Ancient layered sediments in Becquerel crater are actively being carved into flutes and yardangs by the blowing sands. Dunes in an un-named crater in Meridiani near the Mars Exploration Rover Opportunity landing site advanced as much as 50cm over an interval of one Martian year. Copyright (c) 2012 John Wiley & Sons, Ltd.
C1 [Geissler, Paul E.] US Geol Survey, Flagstaff, AZ 86001 USA.
[Stantzos, Nicholas W.] No Arizona Univ, Flagstaff, AZ 86011 USA.
[Bridges, Nathan T.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD USA.
[Bourke, Mary C.] Planetary Sci Inst, Tucson, AZ USA.
[Silvestro, Simone; Fenton, Lori K.] SETI Inst, Mountain View, CA USA.
[Fenton, Lori K.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
RP Geissler, PE (reprint author), US Geol Survey, Ctr Astrogeol, 2255 N Gemini Dr, Flagstaff, AZ 86001 USA.
EM pgeissler@usgs.gov
RI Bourke, Mary/I-4387-2012; Bridges, Nathan/D-6341-2016
OI Bourke, Mary/0000-0002-0424-0322;
FU NASA Mars Data Analysis program [NNH09ZDA001N]
FX The efforts of the science and operations teams of both MER and HiRISE
in acquiring these data are gratefully acknowledged. Figures 1, 2, 5, 6,
and 9 were prepared with JMARS software from Arizona State University.
Thoughtful comments from Robert Sullivan and another reviewer helped
improve the scholarship of this article. S. Silvestro is supported by a
grant from the NASA Mars Data Analysis program (NNH09ZDA001N).
NR 21
TC 8
Z9 8
U1 2
U2 16
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 0197-9337
J9 EARTH SURF PROC LAND
JI Earth Surf. Process. Landf.
PD MAR
PY 2013
VL 38
IS 4
BP 407
EP 412
DI 10.1002/esp.3331
PG 6
WC Geography, Physical; Geosciences, Multidisciplinary
SC Physical Geography; Geology
GA 112DZ
UT WOS:000316573700007
ER
PT J
AU Gatabi, IR
Johnson, DW
Woo, JH
Anderson, JW
Coan, MR
Piner, EL
Harris, HR
AF Gatabi, Iman Rezanezhad
Johnson, Derek W.
Woo, Jung Hwan
Anderson, Jonathan W.
Coan, Mary R.
Piner, Edwin L.
Harris, Harlan Rusty
TI PECVD Silicon Nitride Passivation of AlGaN/GaN Heterostructures
SO IEEE TRANSACTIONS ON ELECTRON DEVICES
LA English
DT Article
DE Gallium nitride; passivation; piezoelectric polarization; spontaneous
polarization
ID RAY PHOTOEMISSION SPECTROSCOPY; ELECTRON-MOBILITY TRANSISTORS;
PIEZOELECTRIC POLARIZATION; QUANTUM-WELLS; WURTZITE GAN; FIELD;
HETEROJUNCTIONS; THICKNESSES; TRANSITION; ALN
AB This paper investigates the optimization of PECVD alpha-SiN-passivated AlGaN/GaN heterostructures to achieve higher 2-D electron gas (2DEG) densities and lower the electric fields residing in the AlGaN barrier layer. A model is developed to calculate the 2DEG density of passivated AlGaN/GaN heterostructures taking into account the piezoelectric and spontaneous polarization effects together with strain relaxation. The model is validated with 2DEG measurements and data from the literature. The optimized passivation layer thickness is calculated for different Al mole fractions and AlGaN thicknesses to achieve targeted 2DEG densities and polarization electric field. Fabrication of samples with different alpha-SiN thicknesses and effects of postannealing on 2DEG density are reported. The model accurately predicts the experimental results.
C1 [Gatabi, Iman Rezanezhad; Johnson, Derek W.; Woo, Jung Hwan; Harris, Harlan Rusty] Texas A&M Univ, Dept Elect & Comp Engn, College Stn, TX 77843 USA.
[Anderson, Jonathan W.; Piner, Edwin L.] SW Texas State Univ, Dept Phys, San Marcos, TX 78666 USA.
[Coan, Mary R.] NASA, John F Kennedy Space Ctr, Kennedy Space Ctr, FL 32899 USA.
[Harris, Harlan Rusty] Texas A&M Univ, Dept Phys, College Stn, TX 77843 USA.
RP Gatabi, IR (reprint author), Texas A&M Univ, Dept Elect & Comp Engn, College Stn, TX 77843 USA.
EM irezanejad@tamu.edu; dwjohnson87@gmail.com; j.woo@tamu.edu;
ja1533@txstate.ed; mcoan2@gmail.com; epiner@txstate.edu;
rusty.harris@tamu.edu
RI Piner, Edwin/B-5359-2016
NR 32
TC 9
Z9 10
U1 0
U2 59
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 0018-9383
EI 1557-9646
J9 IEEE T ELECTRON DEV
JI IEEE Trans. Electron Devices
PD MAR
PY 2013
VL 60
IS 3
BP 1082
EP 1087
DI 10.1109/TED.2013.2242075
PG 6
WC Engineering, Electrical & Electronic; Physics, Applied
SC Engineering; Physics
GA 115NW
UT WOS:000316820000026
ER
PT J
AU Probst, AJ
Holman, HYN
DeSantis, TZ
Andersen, GL
Birarda, G
Bechtel, HA
Piceno, YM
Sonnleitner, M
Venkateswaran, K
Moissl-Eichinger, C
AF Probst, Alexander J.
Holman, Hoi-Ying N.
DeSantis, Todd Z.
Andersen, Gary L.
Birarda, Giovanni
Bechtel, Hans A.
Piceno, Yvette M.
Sonnleitner, Maria
Venkateswaran, Kasthuri
Moissl-Eichinger, Christine
TI Tackling the minority: sulfate-reducing bacteria in an archaea-dominated
subsurface biofilm
SO ISME JOURNAL
LA English
DT Article
DE Archaea; microbial ecology; PhyloChip; SR-FTIR; SRB; CTC
ID PEARLS-LIKE MORPHOLOGY; RIBOSOMAL-RNA; RAMAN MICROSPECTROSCOPY;
PHYLOGENETIC ANALYSIS; NATURAL COMMUNITIES; MASS-SPECTROMETRY; SULFIDIC
SPRINGS; SM1 EURYARCHAEON; MEMBRANE-LIPIDS; MICROBIAL MATS
AB Archaea are usually minor components of a microbial community and dominated by a large and diverse bacterial population. In contrast, the SM1 Euryarchaeon dominates a sulfidic aquifer by forming subsurface biofilms that contain a very minor bacterial fraction (5%). These unique biofilms are delivered in high biomass to the spring outflow that provides an outstanding window to the subsurface. Despite previous attempts to understand its natural role, the metabolic capacities of the SM1 Euryarchaeon remain mysterious to date. In this study, we focused on the minor bacterial fraction in order to obtain insights into the ecological function of the biofilm. We link phylogenetic diversity information with the spatial distribution of chemical and metabolic compounds by combining three different state-of-the-art methods: PhyloChip G3 DNA microarray technology, fluorescence in situ hybridization (FISH) and synchrotron radiation-based Fourier transform infrared (SR-FTIR) spectromicroscopy. The results of PhyloChip and FISH technologies provide evidence for selective enrichment of sulfate-reducing bacteria, which was confirmed by the detection of bacterial dissimilatory sulfite reductase subunit B (dsrB) genes via quantitative PCR and sequence-based analyses. We further established a differentiation of archaeal and bacterial cells by SR-FTIR based on typical lipid and carbohydrate signatures, which demonstrated a co-localization of organic sulfate, carbonated mineral and bacterial signatures in the biofilm. All these results strongly indicate an involvement of the SM1 euryarchaeal biofilm in the global cycles of sulfur and carbon and support the hypothesis that sulfidic springs are important habitats for Earth's energy cycles. Moreover, these investigations of a bacterial minority in an Archaea-dominated environment are a remarkable example of the great power of combining highly sensitive microarrays with label-free infrared imaging. The ISME Journal (2013) 7, 635-651; doi:10.1038/ismej.2012.133; published online 22 November 2012
C1 [Probst, Alexander J.; Sonnleitner, Maria; Moissl-Eichinger, Christine] Univ Regensburg, Inst Microbiol, D-93053 Regensburg, Germany.
[Probst, Alexander J.; Sonnleitner, Maria; Moissl-Eichinger, Christine] Univ Regensburg, Archaea Ctr, D-93053 Regensburg, Germany.
[Probst, Alexander J.; Holman, Hoi-Ying N.; Andersen, Gary L.; Birarda, Giovanni; Piceno, Yvette M.] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Ctr Environm Biotechnol, Berkeley, CA 94720 USA.
[DeSantis, Todd Z.] Second Genome Inc, Dept Bioinformat, San Bruno, CA USA.
[Bechtel, Hans A.] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Adv Light Source, Berkeley, CA 94720 USA.
[Venkateswaran, Kasthuri] CALTECH, Jet Prop Lab, Biotechnol & Planetary Protect Grp, Pasadena, CA USA.
RP Moissl-Eichinger, C (reprint author), Univ Regensburg, Inst Microbiol, Univ Str 31, D-93053 Regensburg, Germany.
EM christine.moissl-eichinger@ur.de
RI Holman, Hoi-Ying/N-8451-2014; Piceno, Yvette/I-6738-2016; Probst,
Alexander/K-2813-2016; Moissl-Eichinger, Christine/A-6682-2015;
Andersen, Gary/G-2792-2015
OI Holman, Hoi-Ying/0000-0002-7534-2625; Piceno,
Yvette/0000-0002-7915-4699; Moissl-Eichinger,
Christine/0000-0001-6755-6263; Andersen, Gary/0000-0002-1618-9827
FU DFG [MO19773-1]; U.S. Department of Energy [DE-AC02-05CH11231]; U.S.
Department of Energy, Office of Science and Office of Biological and
Environmental Research [DE-AC02-05CH11231]; Office of Science, Office of
Basic Energy Sciences, of the U.S. Department of Energy
[DE-AC02-05CH11231]; German National Academic Foundation
(Studienstiftung des deutschen Volkes)
FX Technical assistance by Lauren Tom as well as review and discussion
provided by Robert Huber and Reinhard Wirth are much appreciated. Work
at University of Regensburg was performed under the DFG grant MO19773-1
given to Christine Moissl-Eichinger. Phylogenetic work at Lawrence
Berkeley National Laboratory was performed under the auspices of the
U.S. Department of Energy under contract no. DE-AC02-05CH11231. The
SR-FTIR and associated imaging work were performed under the Berkeley
Synchrotron Infrared Structural Biology (BSISB) Program and the
Subsurface Science Scientific Focus Area funded by the U.S. Department
of Energy, Office of Science and Office of Biological and Environmental
Research through contracts DE-AC02-05CH11231. The Advanced Light Source
is supported by the Director, Office of Science, Office of Basic Energy
Sciences, of the U.S. Department of Energy under contract no.
DE-AC02-05CH11231. The authors are grateful to PreSens (Germany,
Regensburg) for providing the oxygen dipping probe PSt6 and the Fibox 3,
LCD trace. Alexander J Probst was supported by the German National
Academic Foundation (Studienstiftung des deutschen Volkes).
NR 84
TC 18
Z9 19
U1 6
U2 82
PU NATURE PUBLISHING GROUP
PI LONDON
PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND
SN 1751-7362
J9 ISME J
JI ISME J.
PD MAR
PY 2013
VL 7
IS 3
BP 635
EP 651
DI 10.1038/ismej.2012.133
PG 17
WC Ecology; Microbiology
SC Environmental Sciences & Ecology; Microbiology
GA 114FL
UT WOS:000316726400019
PM 23178669
ER
PT J
AU Hitchcock, P
Shepherd, TG
Manney, GL
AF Hitchcock, Peter
Shepherd, Theodore G.
Manney, Gloria L.
TI Statistical Characterization of Arctic Polar-Night Jet Oscillation
Events
SO JOURNAL OF CLIMATE
LA English
DT Article
ID STRATOSPHERIC SUDDEN WARMINGS; MIDDLE ATMOSPHERE MODEL;
NORTHERN-HEMISPHERE; VARIABILITY; TROPOSPHERE; VORTEX; CLIMATOLOGY;
PROPAGATION; CIRCULATION; ANOMALIES
AB A novel diagnostic tool is presented, based on polar-cap temperature anomalies, for visualizing daily variability of the Arctic stratospheric polar vortex over multiple decades. This visualization illustrates the ubiquity of extended-time-scale recoveries from stratospheric sudden warmings, termed here polar-night jet oscillation (PJO) events. These are characterized by an anomalously warm polar lower stratosphere that persists for several months. Following the initial warming, a cold anomaly forms in the middle stratosphere, as does an anomalously high stratopause, both of which descend while the lower-stratospheric anomaly persists. These events are characterized in four datasets: Microwave Limb Sounder (MLS) temperature observations; the 40-yr ECMWF Re-Analysis (ERA-40) and Modern Era Retrospective Analysis for Research and Applications (MERRA) reanalyses; and an ensemble of three 150-yr simulations from the Canadian Middle Atmosphere Model. The statistics of PJO events in the model are found to agree very closely with those of the observations and reanalyses.
The time scale for the recovery of the polar vortex following sudden warmings correlates strongly with the depth to which the warming initially descends. PJO events occur following roughly half of all major sudden warmings and are associated with an extended period of suppressed wave-activity fluxes entering the polar vortex. They follow vortex splits more frequently than they do vortex displacements. They are also related to weak vortex events as identified by the northern annular mode; in particular, those weak vortex events followed by a PJO event show a stronger tropospheric response. The long time scales, predominantly radiative dynamics, and tropospheric influence of PJO events suggest that they represent an important source of conditional skill in seasonal forecasting.
C1 [Hitchcock, Peter; Shepherd, Theodore G.] Univ Toronto, Dept Phys, Toronto, ON, Canada.
[Manney, Gloria L.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Manney, Gloria L.] New Mexico Inst Min & Technol, Socorro, NM 87801 USA.
RP Hitchcock, P (reprint author), Univ Cambridge, Dept Appl Math & Theoret Phys, Wilberforce Rd, Cambridge CB3 0WA, England.
EM aph42@cam.ac.uk
OI Hitchcock, Peter/0000-0001-8993-3808
FU Natural Sciences and Engineering Research Council; Canadian Foundation
for Climate and Atmospheric Sciences
FX We are grateful to Shigeo Yoden for many helpful discussions,
particularly during an extended visit by PH under the Japan Society for
the Promotion of Science summer program. We thank William Daffer for
providing the polar-cap temperature data from MLS, Michael Neish and
Isla Simpson for technical assistance accessing the CMAM model data, and
two anonymous reviewers for their helpful comments. We also acknowledge
the support of the Natural Sciences and Engineering Research Council and
the Canadian Foundation for Climate and Atmospheric Sciences. Work at
the California Institute of Technology Jet Propulsion Laboratory was
done under contract with the National Aeronautics and Space
Administration.
NR 44
TC 28
Z9 28
U1 0
U2 16
PU AMER METEOROLOGICAL SOC
PI BOSTON
PA 45 BEACON ST, BOSTON, MA 02108-3693 USA
SN 0894-8755
J9 J CLIMATE
JI J. Clim.
PD MAR
PY 2013
VL 26
IS 6
BP 2096
EP 2116
DI 10.1175/JCLI-D-12-00202.1
PG 21
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 112UV
UT WOS:000316620500015
ER
PT J
AU Shams, QA
Zuckerwar, AJ
Burkett, CG
Weistroffer, GR
Hugo, DR
AF Shams, Qamar A.
Zuckerwar, Allan J.
Burkett, Cecil G.
Weistroffer, George R.
Hugo, Derek R.
TI Experimental investigation into infrasonic emissions from atmospheric
turbulence
SO JOURNAL OF THE ACOUSTICAL SOCIETY OF AMERICA
LA English
DT Article
ID PROPAGATION; ARRAYS; SOUND; WAVES
AB Clear air turbulence (CAT) is the leading cause of in-flight injuries and in severe cases can result in fatalities. The purpose of this work is to design and develop an infrasonic array network for early warning of clear air turbulence. The infrasonic system consists of an infrasonic three-microphone array, compact windscreens, and data management system. Past experimental efforts to detect acoustic emissions from CAT have been limited. An array of three infrasonic microphones, operating in the field at NASA Langley Research Center, on several occasions received signals interpreted as infrasonic emissions from CAT. Following comparison with current lidar and other past methods, the principle of operation, the experimental methods, and experimental data are presented for case studies and confirmed by pilot reports. The power spectral density of the received signals was found to fit a power law having an exponent of -6 to -7, which is found to be characteristics of infrasonic emissions from CAT, in contrast to findings of the past. [http://dx.doi.org/10.1121/1.4776180]
C1 [Shams, Qamar A.] NASA, Langley Res Ctr, Hampton, VA 23681 USA.
[Zuckerwar, Allan J.; Burkett, Cecil G.; Weistroffer, George R.] Analyt Serv & Mat Inc, Hampton, VA 23666 USA.
[Hugo, Derek R.] Rochester Inst Technol, Rochester, NY 14623 USA.
RP Shams, QA (reprint author), NASA, Langley Res Ctr, Mail Stop 238, Hampton, VA 23681 USA.
EM Qamar.A.Shams@nasa.gov
FU Creativity and Innovation Program; NASA Langley Research Center
FX The authors thank John W. Stoughton for developing the signal processing
algorithms used in the data analysis. This work was supported by the
Creativity and Innovation Program and by the Innovative Partnership
Program at NASA Langley Research Center.
NR 29
TC 3
Z9 3
U1 0
U2 7
PU ACOUSTICAL SOC AMER AMER INST PHYSICS
PI MELVILLE
PA STE 1 NO 1, 2 HUNTINGTON QUADRANGLE, MELVILLE, NY 11747-4502 USA
SN 0001-4966
J9 J ACOUST SOC AM
JI J. Acoust. Soc. Am.
PD MAR
PY 2013
VL 133
IS 3
BP 1269
EP 1280
DI 10.1121/1.4776180
PG 12
WC Acoustics; Audiology & Speech-Language Pathology
SC Acoustics; Audiology & Speech-Language Pathology
GA 108NP
UT WOS:000316300900021
PM 23464000
ER
PT J
AU Jacobson, N
Harder, B
Myers, D
AF Jacobson, Nathan
Harder, Bryan
Myers, Dwight
TI Oxidation Transitions for SiC Part I. Active-to-Passive Transitions
SO JOURNAL OF THE AMERICAN CERAMIC SOCIETY
LA English
DT Article
ID HIGH-TEMPERATURE OXIDATION; SILICON-CARBIDE; PRESSURE; OXYGEN; NITRIDE;
HELIUM; AIR
AB Oxidation of SiC can occur in a passive mode where a protective film is generated or in an active mode where a volatile suboxide is generated and can lead to rapid material consumption. The transition between these two modes of oxidation is a critical issue. Evidence indicates that this transition occurs via a different mechanism for the active-to-passive transition as compared with that of the passive-to-active transition. In Part I of this article, the former (active-to-passive mode) is explored. Three different types of SiC are examined: Si-rich SiC, stoichiometric SiC, and C-rich SiC. Evidence suggests that the SiO2/SiC equilibrium requirements as well as formation of SiO(g) at the SiC surface and subsequent oxidation to SiO2(s) are critical issues in the active-to-passive transition.
C1 [Jacobson, Nathan; Harder, Bryan] NASA Glenn Res Ctr, Cleveland, OH 44135 USA.
[Myers, Dwight] E Cent Univ, Ada, OK 74820 USA.
RP Jacobson, N (reprint author), NASA Glenn Res Ctr, Cleveland, OH 44135 USA.
EM nathan.s.jacobson@nasa.gov
NR 27
TC 19
Z9 20
U1 1
U2 23
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 0002-7820
J9 J AM CERAM SOC
JI J. Am. Ceram. Soc.
PD MAR
PY 2013
VL 96
IS 3
BP 838
EP 844
DI 10.1111/jace.12108
PG 7
WC Materials Science, Ceramics
SC Materials Science
GA 112DJ
UT WOS:000316572000028
ER
PT J
AU Robinson, C
Saatchi, S
Neumann, M
Gillespie, T
AF Robinson, Chelsea
Saatchi, Sassan
Neumann, Maxim
Gillespie, Thomas
TI Impacts of Spatial Variability on Aboveground Biomass Estimation from
L-Band Radar in a Temperate Forest
SO REMOTE SENSING
LA English
DT Article
DE radar; UAVSAR; biomass; forest structure; Maine; Howland
ID SYNTHETIC-APERTURE RADAR; BOREAL FORESTS; BACKSCATTER; INTENSITY;
ECOSYSTEM
AB Estimation of forest aboveground biomass (AGB) has become one of the main challenges of remote sensing science for global observation of carbon storage and changes in the past few decades. We examine the impact of plot size at different spatial resolutions, incidence angles, and polarizations on the forest biomass estimation using L-band polarimetric Synthetic Aperture Radar data acquired by NASA's Unmanned Aerial Vehicle Synthetic Aperture Radar (UAVSAR) airborne system. Field inventory data from 32 1.0 ha plots (AGB < 200 Mg ha(-1)) in approximately even-aged forests in a temperate to boreal transitional region in the state of Maine were divided into subplots at four different spatial scales (0.0625 ha, 0.25 ha, 0.5 ha, and 1.0 ha) to quantify aboveground biomass variations. The results showed a large variability in aboveground biomass at smaller plot size (0.0625 ha). The variability decreased substantially at larger plot sizes (>0.5 ha), suggesting a stability of field-estimated biomass at scales of about 1.0 ha. UAVSAR backscatter was linked to the field estimates of aboveground biomass to develop parametric equations based on polarized returns to accurately map biomass over the entire radar image. Radar backscatter values at all three polarizations (HH, VV, HV) were positively correlated with field aboveground biomass at all four spatial scales, with the highest correlation at the 1.0 ha scale. Among polarizations, the cross-polarized HV had the highest sensitivity to field estimated aboveground biomass (R-2 = 0.68). Algorithms were developed that combined three radar backscatter polarizations (HH, HV, and VV) to estimate aboveground biomass at the four spatial scales. The predicted aboveground biomass from these algorithms resulted in decreasing estimation error as the pixel size increased, with the best results at the 1 ha scale with an R-2 of 0.67 (p < 0.0001), and an overall RMSE of 44 Mg.ha(-1). For AGB < 150 Mg.ha(-1), the error reduced to 23 Mg.ha(-1) (+/- 15%), suggesting an improved AGB prediction below the L-band sensitivity range to biomass. Results also showed larger bias in aboveground biomass estimation from radar at smaller scales that improved at larger spatial scales of 1.0 ha with underestimation of -3.62 Mg.ha(-1) over the entire biomass range.
C1 [Robinson, Chelsea; Gillespie, Thomas] Univ Calif Los Angeles, Dept Geog, Los Angeles, CA 90095 USA.
[Saatchi, Sassan; Neumann, Maxim] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Robinson, C (reprint author), Univ Calif Los Angeles, Dept Geog, Los Angeles, CA 90095 USA.
EM cmrobins@ucla.edu; Sasan.S.Saatchi@jpl.nasa.gov;
Maxim.Neumann@jpl.nasa.gov; tg@geog.ucla.edu
FU UCLA Geography department
FX The authors would like to thank the researchers and staff at the Howland
flux tower site, especially John Lee, David Hollinger, and Bryan Dail.
We would also like to thank the UCLA Geography department for their
support of this research. A special thanks for the crews that helped
with the field collections from UCLA, NASA's Jet Propulsion Laboratory,
NASA's Goddard Space Flight Center, the University of Maryland, and the
University of Maine.
NR 33
TC 24
Z9 24
U1 0
U2 39
PU MDPI AG
PI BASEL
PA POSTFACH, CH-4005 BASEL, SWITZERLAND
SN 2072-4292
J9 REMOTE SENS-BASEL
JI Remote Sens.
PD MAR
PY 2013
VL 5
IS 3
BP 1001
EP 1023
DI 10.3390/rs5031001
PG 23
WC Remote Sensing
SC Remote Sensing
GA 112RY
UT WOS:000316612000001
ER
PT J
AU Hashimoto, H
Wang, WL
Milesi, C
Xiong, J
Ganguly, S
Zhu, ZC
Nemani, RR
AF Hashimoto, Hirofumi
Wang, Weile
Milesi, Cristina
Xiong, Jun
Ganguly, Sangram
Zhu, Zaichun
Nemani, Ramakrishna R.
TI Structural Uncertainty in Model-Simulated Trends of Global Gross Primary
Production
SO REMOTE SENSING
LA English
DT Article
DE GPP; VPD; precipitation; GIMMS 3g; TOPS
ID NET PRIMARY PRODUCTION; DROUGHT-INDUCED REDUCTION; TERRESTRIAL GROSS;
STOMATAL CONTROL; CARBON-DIOXIDE; WATER; ECOSYSTEMS; RADIATION;
NITROGEN; CLIMATE
AB Projected changes in the frequency and severity of droughts as a result of increase in greenhouse gases have a significant impact on the role of vegetation in regulating the global carbon cycle. Drought effect on vegetation Gross Primary Production (GPP) is usually modeled as a function of Vapor Pressure Deficit (VPD) and/or soil moisture. Climate projections suggest a strong likelihood of increasing trend in VPD, while regional changes in precipitation are less certain. This difference in projections between VPD and precipitation can cause considerable discrepancies in the predictions of vegetation behavior depending on how ecosystem models represent the drought effect. In this study, we scrutinized the model responses to drought using the 30-year record of Global Inventory Modeling and Mapping Studies (GIMMS) 3g Normalized Difference Vegetation Index (NDVI) dataset. A diagnostic ecosystem model, Terrestrial Observation and Prediction System (TOPS), was used to estimate global GPP from 1982 to 2009 under nine different experimental simulations. The control run of global GPP increased until 2000, but stayed constant after 2000. Among the simulations with single climate constraint (temperature, VPD, rainfall and solar radiation), only the VPD-driven simulation showed a decrease in 2000s, while the other scenarios simulated an increase in GPP. The diverging responses in 2000s can be attributed to the difference in the representation of the impact of water stress on vegetation in models, i.e., using VPD and/or precipitation. Spatial map of trend in simulated GPP using GIMMS 3g data is consistent with the GPP driven by soil moisture than the GPP driven by VPD, confirming the need for a soil moisture constraint in modeling global GPP.
C1 [Hashimoto, Hirofumi; Wang, Weile; Milesi, Cristina] Calif State Univ Monterey Bay, Div Sci & Environm Policy, Seaside, CA 93955 USA.
[Hashimoto, Hirofumi; Wang, Weile; Milesi, Cristina; Xiong, Jun; Ganguly, Sangram; Nemani, Ramakrishna R.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Ganguly, Sangram] Bay Area Environm Res Inst, Sonoma, CA 95476 USA.
[Zhu, Zaichun] Boston Univ, Dept Earth & Environm, Boston, MA 02215 USA.
[Zhu, Zaichun] Beijing Normal Univ, Coll Resources Sci & Technol, State Key Lab Earth Proc & Resource Ecol, Beijing 100875, Peoples R China.
RP Hashimoto, H (reprint author), Calif State Univ Monterey Bay, Div Sci & Environm Policy, Seaside, CA 93955 USA.
EM hirofumi.hashimoto@gmail.com; weile.wang@gmail.com;
sangramganguly@gmail.com; zhu.zaichum@gmail.com; rama.nemani@nasa.gov
RI ganguly, sangram/B-5108-2010
FU NASA
FX We wish to thank Compton J. Tucker, Jorge E. Pinzon, and Molly E. Brown
for providing GIMMS 3g datasets. This study was funded by NASA's Earth
Sciences Program. This research was performed using NASA Earth Exchange.
NEX combines state-of-the-art supercomputing, Earth system modeling,
remote sensing data from NASA and other agencies, and a scientific
social networking platform to deliver a complete work environment in
which users can explore and analyze large Earth science data sets, run
modeling codes, collaborate on new or existing projects, and share
results within and/or among communities.
NR 50
TC 11
Z9 11
U1 6
U2 34
PU MDPI AG
PI BASEL
PA POSTFACH, CH-4005 BASEL, SWITZERLAND
SN 2072-4292
J9 REMOTE SENS-BASEL
JI Remote Sens.
PD MAR
PY 2013
VL 5
IS 3
BP 1258
EP 1273
DI 10.3390/rs5031258
PG 16
WC Remote Sensing
SC Remote Sensing
GA 112RY
UT WOS:000316612000013
ER
PT J
AU Watkins, T
Bilheux, H
An, K
Payzant, A
Dehoff, R
Duty, C
Peter, W
Blue, C
Brice, C
AF Watkins, Thomas
Bilheux, Hassina
An, Ke
Payzant, Andrew
Dehoff, Ryan
Duty, Chad
Peter, William
Blue, Craig
Brice, Craig
TI Neutron Characterization for Additive Manufacturing
SO ADVANCED MATERIALS & PROCESSES
LA English
DT Article
C1 [Watkins, Thomas; Bilheux, Hassina; An, Ke; Payzant, Andrew; Dehoff, Ryan; Duty, Chad; Peter, William; Blue, Craig] Oak Ridge Natl Lab, Oak Ridge, TN USA.
[Brice, Craig] NASA, Langley Res Ctr, Hampton, VA 23665 USA.
RP Watkins, T (reprint author), ORNL, MS&T Div, Scattering & Thermophys Grp, Oak Ridge, TN USA.
EM watkinstr@ornl.gov
RI Payzant, Edward/B-5449-2009; Bilheux, Hassina/H-4289-2012; An,
Ke/G-5226-2011; Watkins, Thomas/D-8750-2016; Dehoff, Ryan/I-6735-2016
OI Payzant, Edward/0000-0002-3447-2060; Bilheux,
Hassina/0000-0001-8574-2449; An, Ke/0000-0002-6093-429X; Watkins,
Thomas/0000-0002-2646-1329; Dehoff, Ryan/0000-0001-9456-9633
FU U.S. DOE, Office of Energy Efficiency and Renewable Energy, Advanced
Manufacturing Office [DE-AC05-00OR22725]; UT-Battelle LLC.; Scientific
User Facilities Div., Office of Basic Energy Sciences, Department of
Energy
FX Research sponsored by the U.S. DOE, Office of Energy Efficiency and
Renewable Energy, Advanced Manufacturing Office, under contract
DE-AC05-00OR22725 with UT-Battelle LLC. Research conducted at ORNL's
High Flux Isotope Reactor and Spoliation Neutron Source was sponsored by
the Scientific User Facilities Div., Office of Basic Energy Sciences,
Department of Energy.
NR 8
TC 11
Z9 11
U1 5
U2 45
PU ASM INT
PI MATERIALS PARK
PA SUBSCRIPTIONS SPECIALIST CUSTOMER SERVICE, MATERIALS PARK, OH 44073-0002
USA
SN 0882-7958
J9 ADV MATER PROCESS
JI Adv. Mater. Process.
PD MAR
PY 2013
VL 171
IS 3
BP 23
EP 27
PG 5
WC Materials Science, Multidisciplinary
SC Materials Science
GA 106SX
UT WOS:000316166100004
ER
PT J
AU Martinuzzi, S
Gould, WA
Vierling, LA
Hudak, AT
Nelson, RF
Evans, JS
AF Martinuzzi, Sebastian
Gould, William A.
Vierling, Lee A.
Hudak, Andrew T.
Nelson, Ross F.
Evans, Jeffrey S.
TI Quantifying Tropical Dry Forest Type and Succession: Substantial
Improvement with LiDAR
SO BIOTROPICA
LA English
DT Article
DE ALS; biodiversity; land-use legacy; secondary forests; vegetation
structure
ID MULTI-SEASON NDVI; PUERTO-RICO; IMAGING SPECTROSCOPY; RESEARCH
PRIORITIES; SATELLITE IMAGERY; FOOTPRINT LIDAR; IKONOS IMAGERY;
RAIN-FORESTS; LANDSCAPE; USA
AB Improved technologies are needed to advance our knowledge of the biophysical and human factors influencing tropical dry forests, one of the world's most threatened ecosystems. We evaluated the use of light detection and ranging (LiDAR) data to address two major needs in remote sensing of tropical dry forests, i.e., classification of forest types and delineation of forest successional status. We evaluated LiDAR-derived measures of three-dimensional canopy structure and subcanopy topography using classification-tree techniques to separate different dry forest types and successional stages in the Guanica Biosphere Reserve in Puerto Rico. We compared the LiDAR-based results with classifications made from commonly used remote sensing data, including Landsat satellite imagery and radar-based topographic data. The accuracy of the LiDAR-based forest type classification (including native- and exotic-dominated forest classes) was substantially higher than those from previously available data (kappa=0.90 and 0.63, respectively). The best result was obtained when combining LiDAR-derived metrics of canopy structure and topography, and adding Landsat spectral data did not improve the classification. For the second objective, we observed that LiDAR-derived variables of vegetation structure were better predictors of forest successional status (i.e., mid-secondary, late-secondary, and primary forests) than was spectral information from Landsat. Importantly, the key LiDAR predictors identified within each classification-tree model agreed with previous ecological knowledge of these forests. Our study highlights the value of LiDAR remote sensing for assessing tropical dry forests, reinforcing the potential for this novel technology to advance research and management of tropical forests in general. Resumo Nuevas tecnologias son necesarias para avanzar en el conocimiento de los factores biofisicos y humanos que afectan a los bosques tropicales secos, uno de los ecosistemas mas amenazados del mundo. En este estudio evaluamos el uso de la tecnologia LiDAR (light detection and ranging) para cubrir dos limitaciones importantes en la teledeteccion de los bosques tropicales secos, incluidas la clasificacion de los tipos de bosques y la delimitacion de estados sucesionales. Especificamente, evaluamos el potencial de las variables tridimensionales de la estructural del bosque y la topografia derivados de LiDAR, mediante tecnicas de arboles de clasificacion, para separar distintos tipos de bosques y estados sucesionales en la Reserva de Biosfera de Guanica, en Puerto Rico. Comparamos los resultados obtenidos de LiDAR con aquellos derivados de fuentes de datos de sensores remotos comunmente utilizados, como las imagenes Landsat y datos topograficos de radar. La precision de la clasificacion de los tipos de bosques obtenida con LiDAR (incluida la presencia de clases dominadas por especies nativas asi como exoticas) fue sustancialmente superior a aquella obtenida con datos de los otros sensores (kappa=0.90 y 0.63 respectivamente). El mejor resultado se obtuvo al combinar variables estructurales del dosel y topografia, todas ellas de LiDAR. La incorporacion de informacion espectral de las imagenes Landsat no mejoro la clasificacion. Como parte del segundo objetivo, encontramos que las variables estructurales de vegetacion de LiDAR lograron separar los estados sucesionales (bosques secundario tardio, medio, y bosque primario), en una forma superior a los datos espectrales de Landsat.
Importante, las variables de LiDAR identificadas mediante los modelos de clasificacion como las mas importantes en nuestro estudio, concordaron con aquellas esperadas en base al conocimiento ecologico previo de estos bosques. Nuestro trabajo muestra el valor de la tecnologia LiDAR para el estudio de los bosques tropicales secos, y resalta el potencial de esta tecnologia para avanzar en el manejo y la investigacion de los bosques tropicales en general.
C1 [Martinuzzi, Sebastian; Vierling, Lee A.] Univ Idaho, Geospatial Lab Environm Dynam, Dept Forest Ecol & Biogeosci, Moscow, ID 83843 USA.
[Gould, William A.] US Forest Serv, Int Inst Trop Forestry, Rio Piedras, PR 00926 USA.
[Hudak, Andrew T.] US Forest Serv, Rocky Mt Res Stn, Moscow, ID 83843 USA.
[Nelson, Ross F.] NASA, Goddard Space Flight Ctr, Biospher Sci Branch, Greenbelt, MD 20771 USA.
[Evans, Jeffrey S.] Nature Conservancy, North Amer Reg Sci, Ft Collins, CO 80524 USA.
RP Martinuzzi, S (reprint author), Univ Wisconsin, Dept Forest & Wildlife Ecol, Madison, WI 53706 USA.
EM martinuzzi@wisc.edu
RI Vierling, Lee/E-6428-2010; Nelson, Ross/H-8266-2014;
OI Vierling, Lee/0000-0001-5344-1983; Evans, Jeffrey/0000-0002-5533-7044;
Gould, William/0000-0002-3720-9735
FU USGS Gap Analysis Program
FX This study was funded by the USGS Gap Analysis Program. E. Naesset, M.
Falkowski, and J. Stoker provided valuable inputs in early stages of
this study. R. Agosto, E. Medina, J. Chinea, and S. Van Bloem
facilitated field information. Technical support was provided by the
University of Idaho, the U.S. Forest Service Moscow Forest Science
Laboratory and the U.S. Forest Service IITF. Study at IITF is conducted
in collaboration with the University of Puerto Rico.
NR 79
TC 5
Z9 5
U1 7
U2 75
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 0006-3606
J9 BIOTROPICA
JI Biotropica
PD MAR
PY 2013
VL 45
IS 2
BP 135
EP 146
DI 10.1111/j.1744-7429.2012.00904.x
PG 12
WC Ecology
SC Environmental Sciences & Ecology
GA 099TE
UT WOS:000315643900001
ER
PT J
AU Lee, J
Worden, J
Koh, DC
Yoshimura, K
Lee, JE
AF Lee, Jeonghoon
Worden, John
Koh, Dong-Chan
Yoshimura, Kei
Lee, Jung-Eun
TI A seasonality of delta D of water vapor (850-500 hPa) observed from
space over Jeju Island, Korea
SO GEOSCIENCES JOURNAL
LA English
DT Article
DE Jeju Island; isotope; water vapor; seasonality
ID VOLCANIC ISLAND; ENVIRONMENTAL ISOTOPES; PRECIPITATION; ASIA; BIAS; TES
AB We examined the seasonal variations of isotopic composition of water vapor in the lower troposphere (850-500 hPa) to relate those of precipitation and groundwater using satellite observations from the Aura Tropospheric Emission Spectrometer (TES) over the volcanic Island of Jeju, Korea. We ran an isotope-enabled general circulation model (IsoGSM) and calculated 120-hr reverse-calculated trajectories for air parcels corresponding to the TES observations to better understand the seasonal variations of delta D of water vapor in the lower troposphere. delta D of precipitation by previous studies and the model results show winter-enriched, while summer-enriched water vapor isotope is observed by the TES observations, which may require a validation campaign using in-situ measurements or continuous monitoring of water vapor isotopes around Jeju Island.
C1 [Lee, Jeonghoon; Worden, John; Lee, Jung-Eun] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Lee, Jeonghoon] Korea Polar Res Inst, Inchon 406840, South Korea.
[Koh, Dong-Chan] Korea Inst Geoscience & Mineral Resources, Taejon 305350, South Korea.
[Yoshimura, Kei] Univ Tokyo, Atmospher & Ocean Res Inst, Chiba 2778568, Japan.
RP Lee, J (reprint author), Ewha Womans Univ, Dept Sci Educ, Seoul 120750, South Korea.
EM jeonghoon.d.lee@gmail.com
RI Yoshimura, Kei/F-2041-2010; Lee, Jeonghoon/E-8116-2010
OI Yoshimura, Kei/0000-0002-5761-1561; Lee, Jeonghoon/0000-0002-1256-4431
FU KOPRI [PE12070]
FX The research described in this paper was carried out at the Jet
Propulsion Laboratory, California Institute of Technology, under a
contract with the National Aeronautics and Space Administration. This
work was partially supported by KOPRI research grant (PE12070). Valuable
comments from an anonymous reviewer and Dr. Kwang-Sik Lee have improved
the quality of this paper.
NR 36
TC 5
Z9 5
U1 0
U2 13
PU GEOLOGICAL SOCIETY KOREA
PI SEOUL
PA NEW BLD RM 813, KSTC, 835-4, YEOKSAM-DONG, KANGNAM-GU, SEOUL, 135-703,
SOUTH KOREA
SN 1226-4806
J9 GEOSCI J
JI Geosci. J.
PD MAR
PY 2013
VL 17
IS 1
BP 87
EP 95
DI 10.1007/s12303-013-0003-5
PG 9
WC Geosciences, Multidisciplinary
SC Geology
GA 106DK
UT WOS:000316121900009
ER
PT J
AU Villanueva, GL
Mumma, MJ
Novak, RE
Radeva, YL
Kaufl, HU
Smette, A
Tokunaga, A
Khayat, A
Encrenaz, T
Hartogh, P
AF Villanueva, G. L.
Mumma, M. J.
Novak, R. E.
Radeva, Y. L.
Kaeufl, H. U.
Smette, A.
Tokunaga, A.
Khayat, A.
Encrenaz, T.
Hartogh, P.
TI A sensitive search for organics (CH4, CH3OH, H2CO, C2H6, C2H2, C2H4),
hydroperoxyl (HO2), nitrogen compounds (N2O, NH3, HCN) and chlorine
species (HCl, CH3Cl) on Mars using ground-based high-resolution infrared
spectroscopy
SO ICARUS
LA English
DT Article
DE Mars, Atmosphere; Organic chemistry; Astrobiology; Spectroscopy;
Infrared observations
ID CHEMICAL PATHWAY ANALYSIS; X-RAY SPECTROMETER; MARTIAN ATMOSPHERE;
ISOTOPIC FRACTIONATION; MINOR CONSTITUENTS; HYDROGEN-PEROXIDE; SURFACE
SAMPLES; SCATTERED-LIGHT; UPPER LIMITS; MU-M
AB Is Mars actively releasing organic and other minor gases into the atmosphere? We present a comprehensive search for trace species on Mars, targeting multiple volatile organic species (CH4, CH3OH, H2CO, C2H6, C2H2, C2H4), hydroperoxyl (HO2), several nitrogen compounds (N2O, NH3, HCN), and two chlorine species (HCl, CH3Cl) through their rovibrational spectra in the 2.8-3.7 mu m spectral region. The data were acquired over a period of 4 years (2006-2010) using powerful infrared high-resolution spectrometers (CRIRES, NIRSPEC, CSHELL) at high-altitude observatories (VLT, Keck-2, NASA-IRTF), and span a broad range of seasons, Doppler shifts and spatial coverage. Here, we present results from a selection of high-quality spectra obtained on four separate dates, representing a fraction of our search space. For most of these species we derived the most stringent upper limits ever obtained, and because the targeted gases have substantially different resident lifetimes in the Martian atmosphere (from hours to centuries), our measurements not only test for current release but also provide stringent limits on the quiescent levels. In particular, we sampled the same regions where plumes of methane have been recently observed (e.g., Syrtis Major and Valles Marineris), allowing us to test for seasonal and temporal variability. (C) 2012 Elsevier Inc. All rights reserved.
C1 [Villanueva, G. L.; Mumma, M. J.; Radeva, Y. L.] NASA, Solar Syst Explorat Div, Goddard Space Flight Ctr, Mailstop 690, Greenbelt, MD 20771 USA.
[Villanueva, G. L.; Radeva, Y. L.] Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA.
[Novak, R. E.] Iona Coll, Dept Phys, New Rochelle, NY 10801 USA.
[Kaeufl, H. U.] European So Observ, Munich, Germany.
[Smette, A.] European So Observ, Santiago 19, Chile.
[Tokunaga, A.; Khayat, A.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA.
[Encrenaz, T.] Observ Paris Site Meudon, LEISA, F-92195 Meudon, France.
[Hartogh, P.] Max Planck Inst Solar Syst Res, D-37191 Katlenburg Lindau, Germany.
RP Villanueva, GL (reprint author), NASA, Solar Syst Explorat Div, Goddard Space Flight Ctr, Mailstop 690, Greenbelt, MD 20771 USA.
EM Geronimo.Villanueva@nasa.gov
RI mumma, michael/I-2764-2013
FU NASA [08-PAST08-0034, 08-PATM08-0031, RTOP 344-32-07, RTOP 344-53-51];
NSF-RUI [AST-0805540]; NASA; W.M. Keck Foundation
FX We thank the staff of the Very Large Telescope (VLT), the NASA Infra Red
Telescope Facility (IRTF) and the W.M. Keck Observatory for their
exceptional support throughout our long Mars observing Programs. G.L.V.
acknowledges support from NASA's Planetary Astronomy Program
(08-PAST08-0034) and NASA's Planetary Atmospheres Program
(08-PATM08-0031). NASA's Planetary Astronomy Program (RTOP 344-32-07)
and NASA's Astrobiology Program (RTOP 344-53-51) supported M.J.M., G.L.V
and Y.L.R. NSF-RUI supported REN through Grant (AST-0805540). This work
was also supported by a NASA Keck PI Data Award, administered by the
NASA Exoplanet Science Institute. Data acquired at the W.M. Keck
Observatory utilized telescope time allocated to the National
Aeronautics and Space Administration through the agency's scientific
partnership with the California Institute of Technology and the
University of California. The Observatory was made possible by the
generous financial support of the W.M. Keck Foundation. The authors wish
to recognize and acknowledge the very significant cultural role and
reverence that the summit of Mauna Kea has always had within the
indigenous Hawaiian community. We are most fortunate to have the
opportunity to conduct observations from this mountain.
NR 102
TC 33
Z9 33
U1 0
U2 67
PU ACADEMIC PRESS INC ELSEVIER SCIENCE
PI SAN DIEGO
PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA
SN 0019-1035
EI 1090-2643
J9 ICARUS
JI Icarus
PD MAR
PY 2013
VL 223
IS 1
BP 11
EP 27
DI 10.1016/j.icarus.2012.11.013
PG 17
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 104FP
UT WOS:000315977600002
ER
PT J
AU Neish, CD
Kirk, RL
Lorenz, RD
Bray, VJ
Schenk, P
Stiles, BW
Turtle, E
Mitchell, K
Hayes, A
AF Neish, C. D.
Kirk, R. L.
Lorenz, R. D.
Bray, V. J.
Schenk, P.
Stiles, B. W.
Turtle, E.
Mitchell, K.
Hayes, A.
CA Cassini RADAR Team
TI Crater topography on Titan: Implications for landscape evolution
SO ICARUS
LA English
DT Article
DE Cratering; Titan; Ganymede
ID CASSINI RADAR OBSERVATIONS; GALILEAN SATELLITES; IMPACT CRATER; HUYGENS
PROBE; CENTRAL PEAK; SURFACE; ATMOSPHERE; GANYMEDE; METHANE; LOCKNE
AB We present a comprehensive review of available crater topography measurements for Saturn's moon Titan. In general, the depths of Titan's craters are within the range of depths observed for similarly sized fresh craters on Ganymede, but several hundreds of meters shallower than Ganymede's average depth vs. diameter trend. Depth-to-diameter ratios are between 0.0012 +/- 0.0003 (for the largest crater studied, Menrva, D similar to 425 km) and 0.017 +/- 0.004 (for the smallest crater studied, Ksa, D similar to 39 km). When we evaluate the Anderson-Darling goodness-of-fit parameter, we find that there is less than a 10% probability that Titan's craters have a current depth distribution that is consistent with the depth distribution of fresh craters on Ganymede. There is, however, a much higher probability that the relative depths are uniformly distributed between 0 (fresh) and I (completely infilled). This distribution is consistent with an infilling process that is relatively constant with time, such as aeolian deposition. Assuming that Ganymede represents a close 'airless' analogue to Titan, the difference in depths represents the first quantitative measure of the amount of modification that has shaped Titan's surface, the only body in the outer Solar System with extensive surface-atmosphere exchange. (C) 2012 Elsevier Inc. All rights reserved.
C1 [Neish, C. D.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Kirk, R. L.] US Geol Survey, Astrogeol Sci Ctr, Flagstaff, AZ 86001 USA.
[Lorenz, R. D.; Turtle, E.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA.
[Bray, V. J.] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA.
[Schenk, P.] Lunar & Planetary Inst, Houston, TX 77058 USA.
[Stiles, B. W.; Mitchell, K.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Hayes, A.] Univ Calif Berkeley, Berkeley, CA 94720 USA.
RP Neish, CD (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
EM catherine.d.neish@nasa.gov
RI Neish, Catherine/G-6321-2012; Hayes, Alexander/P-2024-2014; Turtle,
Elizabeth/K-8673-2012; Lorenz, Ralph/B-8759-2016
OI Hayes, Alexander/0000-0001-6397-2630; Turtle,
Elizabeth/0000-0003-1423-5751; Lorenz, Ralph/0000-0001-8528-4644
FU Cassini Project; Miller Institute for Basic Research in Science; NASA;
National Aeronautics and Space Administration
FX We wish to acknowledge the Cassini RADAR Team for acquiring and
processing the data presented here. C.N., R.K., R.L., B.S., and E.T.
further thank the Cassini Project for financial support. A.H. was funded
by the Miller Institute for Basic Research in Science. This work was
also partially supported by an appointment to the NASA Postdoctoral
Program at the Goddard Space Flight Center, administered by Oak Ridge
Associated Universities through a contract with NASA to C.N., and a
portion of this research was carried out at the Jet Propulsion
Laboratory, California Institute of Technology, under a Contract with
the National Aeronautics and Space Administration. We thank O. Abramov
and two anonymous reviewers for comments that helped to improve the
manuscript.
NR 54
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PI SAN DIEGO
PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA
SN 0019-1035
J9 ICARUS
JI Icarus
PD MAR
PY 2013
VL 223
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BP 82
EP 90
DI 10.1016/j.icarus.2012.11.030
PG 9
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 104FP
UT WOS:000315977600009
ER
PT J
AU Hedman, MM
Nicholson, PD
Cuzzi, JN
Clark, RN
Filacchione, G
Capaccioni, F
Ciarniello, M
AF Hedman, M. M.
Nicholson, P. D.
Cuzzi, J. N.
Clark, R. N.
Filacchione, G.
Capaccioni, F.
Ciarniello, M.
TI Connections between spectra and structure in Saturn's main rings based
on Cassini VIMS data
SO ICARUS
LA English
DT Article
DE Planetary rings; Saturn, Rings; Spectroscopy; Ices, IR spectroscopy
ID REFLECTANCE SPECTROSCOPY; SURFACE-COMPOSITION; PLANETARY RING; DUST
GRAINS; SATELLITES; PHOTOMETRY; SCATTERING; PARTICLES; EVOLUTION; ALBEDO
AB Saturn's main rings exhibit variations in both their opacity and their spectral properties on a broad range of spatial scales, and the correlations between these parameters can provide insights into the processes that shape the composition and dynamics of the rings. The Visual and Infrared Mapping Spectrometer (VIMS) instrument onboard the Cassini Spacecraft has obtained spectra of the rings between 0.35 and 5.2 mu m with sufficient spatial resolution to discern variations on scales below 200 km. These relatively high-resolution spectral data reveal that both the depths of the near-infrared water-ice absorption bands and the visible spectral slopes are often correlated with structural parameters such as the rings' optical depth. Using a simplified model for the ring-particles' regolith properties, we have begun to disentangle the trends due to changes in the gross composition of the ring particles from those that may be due to shifts in the texture of the ring particles' regolith. Consistent with previous studies, this analysis finds that the C ring and the Cassini Division possess enhanced concentrations of a contaminant that absorbs light over a broad range of wavelengths. On the other hand, a second contaminant that preferentially absorbs at short visible and near-ultraviolet wavelengths is found to be more evenly distributed throughout the rings. The optical activity of this short-wavelength absorber increases inwards of 100,000 km from Saturn center, which may provide clues to the origin of this contaminant. The spectral variations identified as shifts in the regolith texture are in some places clearly correlated with the ring's optical depth, and in other locations they appear to be associated with the disturbances generated by strong mean-motion resonances with Saturn's various moons. These variations therefore seem to be controlled by the ring particles' dynamical environment, and may even provide a new avenue for constraining the structure and mass density of Saturn's most opaque ring regions. (C) 2013 Published by Elsevier Inc.
C1 [Hedman, M. M.; Nicholson, P. D.] Cornell Univ, Dept Astron, Ithaca, NY 14853 USA.
[Cuzzi, J. N.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Clark, R. N.] US Geol Survey, Denver Fed Ctr, Denver, CO 80225 USA.
[Filacchione, G.; Capaccioni, F.; Ciarniello, M.] INAF IAPS Tor Vergata, I-00133 Rome, Italy.
RP Hedman, MM (reprint author), Cornell Univ, Dept Astron, 322 Space Sci Bldg, Ithaca, NY 14853 USA.
EM mmhedman@astro.cornell.edu
OI Capaccioni, Fabrizio/0000-0003-1631-4314; Filacchione,
Gianrico/0000-0001-9567-0055; Ciarniello, Mauro/0000-0002-7498-5207
FU VIMS team; Cassini Project; NASA
FX We acknowledge the support of the VIMS team, the Cassini Project and
NASA. We would like to thank P. Helfenstein for some useful
conversations regarding this work. We also thank S. Brooks and an
anonymous reviewer for their comments that helped improve this
manuscript.
NR 54
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PI SAN DIEGO
PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA
SN 0019-1035
EI 1090-2643
J9 ICARUS
JI Icarus
PD MAR
PY 2013
VL 223
IS 1
BP 105
EP 130
DI 10.1016/j.icarus.2012.10.014
PG 26
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 104FP
UT WOS:000315977600011
ER
PT J
AU Kramer, GY
Kring, DA
Nahm, AL
Pieters, CM
AF Kramer, Georgiana Y.
Kring, David A.
Nahm, Amanda L.
Pieters, Carle M.
TI Spectral and photogeologic mapping of Schrodinger Basin and implications
for post-South Pole-Aitken impact deep subsurface stratigraphy
SO ICARUS
LA English
DT Article
DE Moon; Spectroscopy; Mineralogy; Impact processes; Geological processes
ID REFLECTANCE SPECTRA; SURFACE DEFORMATION; INFRARED SPECTRA; LUNAR
CRATERS; MOON; MANTLE; SPECTROSCOPY; CLEMENTINE; REGION; MINERALOGY
AB Schrodinger Basin provides a window into the stratigraphy of the lunar crust adjacent to the South Pole-Aitken Basin region that we have probed with Lunar Reconnaissance Orbiter, Moon Mineralogy Mapper (M-3), and crater-scaling relationships. The composition of materials that make up the basin wall, impact melt, and peak ring provide a cross-section of the lunar crust, which reveals products of the lunar magma ocean, subsequent magmatism, and reworking of those components into a megaregolith. Large hectometer- to kilometer-size areas of anorthite-rich material (anorthosite), low-Ca pyroxene material (a noritic unit), and olivine-rich material (troctolite or dunite) are exposed, with a few areas of intermediate composition. The Schrodinger impact excavated similar to 20 km into an orthopyroxene + plagioclase (noritic) lunar crust, which is exposed in the basin walls, rim, and proximal ejecta, and dominates the composition of materials that make up the basin floor. Substantially later in lunar history, two spatially and chronologically isolated volcanic eruptions occurred on the basin floor. Two large craters east of Schrodinger excavated a compositionally gabbroic subsurface unit that was not tapped by Schrodinger. This indicates a compositional crustal facies change, which may be from SPA ejecta, but could reflect heterogeneity in the original lunar crust. (C) 2012 Elsevier Inc. All rights reserved.
C1 [Kramer, Georgiana Y.; Kring, David A.] Lunar & Planetary Inst, Ctr Lunar Sci & Explorat, Houston, TX 77058 USA.
[Nahm, Amanda L.] Univ Texas El Paso, Dept Geol Sci, El Paso, TX 79968 USA.
[Pieters, Carle M.] Brown Univ, Dept Geol Sci, Providence, RI 02912 USA.
[Kramer, Georgiana Y.; Kring, David A.; Pieters, Carle M.] NASA, Lunar Sci Inst, Washington, DC USA.
RP Kramer, GY (reprint author), Lunar & Planetary Inst, Ctr Lunar Sci & Explorat, 3600 Bay Area Blvd, Houston, TX 77058 USA.
EM kramer@lpi.usra.edu
RI Nahm, Amanda/F-4602-2011
OI Nahm, Amanda/0000-0002-3771-6825
FU NASA Lunar Science Institute at the Lunar and Planetary Institute
[NNA09DB33A]; NASA Lunar Science Institute at Brown University
[NNA09DB34A]
FX We thank Teemu Ohman for his numerous contributions to this work
including crater scaling calculations, image processing, references,
editing, and mostly the countless hours spent discussing results,
interpretations, and cross-field integration. We thank Ross Potter for
discussions of the SPA basin-forming event. Both reviewers gave
thoughtful feedback and suggestions that truly improved the manuscript,
and for this the authors are sincerely grateful. This work was supported
by the NASA Lunar Science Institute at the Lunar and Planetary
Institute, Contract #NNA09DB33A (PI DAK) and, in part, by the NASA Lunar
Science Institute at Brown University, Contract #NNA09DB34A (PI CMP).
This is LPI Contribution No. #1705.
NR 88
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PI SAN DIEGO
PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA
SN 0019-1035
EI 1090-2643
J9 ICARUS
JI Icarus
PD MAR
PY 2013
VL 223
IS 1
BP 131
EP 148
DI 10.1016/j.icarus.2012.11.008
PG 18
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 104FP
UT WOS:000315977600012
ER
PT J
AU Kite, ES
Halevy, I
Kahre, MA
Wolff, MJ
Manga, M
AF Kite, Edwin S.
Halevy, Itay
Kahre, Melinda A.
Wolff, Michael J.
Manga, Michael
TI Seasonal melting and the formation of sedimentary rocks on Mars, with
predictions for the Gale Crater mound
SO ICARUS
LA English
DT Article
DE Mars, Climate; Mars, Surface; Mars, Atmosphere; Geological processes;
Mars
ID GENERAL-CIRCULATION MODEL; THERMAL EMISSION SPECTROMETER;
COLLISION-INDUCED ABSORPTION; POLAR LAYERED DEPOSITS; MCMURDO SOUND
REGION; PHOENIX LANDING SITE; MAWRTH-VALLIS REGION; MERIDIANI-PLANUM;
LIQUID WATER; CLIMATE-CHANGE
AB A model for the formation and distribution of sedimentary rocks on Mars is proposed. In this model (ISEE-Mars), the rate-limiting step is supply of liquid water from seasonal melting of snow or ice. The model is run for a O(10(2)) mbar pure CO2 atmosphere, dusty snow, and solar luminosity reduced by 23%. For these conditions snow melts only near the equator, when obliquity and eccentricity are high, and when perihelion occurs near equinox. These requirements for melting are satisfied by 0.01-20% of the probability distribution of Mars' past spin-orbit parameters. This fraction is small, consistent with the geologic record of metastable surface liquid water acting as a "wet-pass filter" of Mars climate history, only recording orbital conditions that permitted surface liquid water. Total melt production is sufficient to account for observed aqueous alteration. The pattern of seasonal snowmelt is integrated over all spin-orbit parameters and compared to the observed distribution of sedimentary rocks. The global distribution of snowmelt has maxima in Valles Marineris, Meridiani Planum and Gale Crater. These correspond to maxima in the sedimentary-rock distribution. Higher pressures and especially higher temperatures lead to melting over a broader range of spin-orbit parameters. The pattern of sedimentary rocks on Mars is most consistent with a model Mars paleoclimate that only rarely produced enough meltwater to precipitate aqueous cements (sulfates, carbonates, phyllosilicates and silica) and indurate sediment. This is consistent with observations suggesting that surface aqueous alteration on Mars was brief and at low water/rock ratio. The results suggest intermittency of snowmelt and long globally-dry intervals, unfavorable for past life on Mars. This model makes testable predictions for the Mars Science Laboratory Curiosity rover at Gale Crater's mound (Mount Sharp, Aeolis Mons). Gale Crater's mound is predicted to be a hemispheric maximum for snowmelt on Mars. (C) 2012 Elsevier Inc. All rights reserved.
C1 [Kite, Edwin S.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA.
[Halevy, Itay] Weizmann Inst Sci, Dept Environm Sci, IL-76100 Rehovot, Israel.
[Kahre, Melinda A.] NASA, Ames Res Ctr, Mountain View, CA 94035 USA.
[Wolff, Michael J.] Space Sci Inst, Boulder, CO 80301 USA.
[Manga, Michael] Univ Calif Berkeley, Dept Earth & Planetary Sci, Berkeley, CA 94720 USA.
[Manga, Michael] Univ Calif Berkeley, Ctr Integrat Planetary Sci, Berkeley, CA 94720 USA.
RP Kite, ES (reprint author), CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA.
EM ekite@caltech.edu
RI Manga, Michael/D-3847-2013; HALEVY, ITAY/K-1364-2012;
OI HALEVY, ITAY/0000-0002-7325-8139; Manga, Michael/0000-0003-3286-4682
FU U.S. taxpayer through NASA [NNX08AN13G, NNX09AN18G, NNX09AL20G,
NNX11AF51G]; NSF [TG-EAR100023]; Weizmann Institute of Science; Israeli
Committee for Higher Education; Caltech; O.K. Earl Fellowship
FX It is a pleasure to thank the following people for their generosity with
time, ideas and data. We are grateful to Richard Brandt and Steve Warren
for sharing the radiation code underlying (Brandt and Warren, 1993).
Paul Niles and anonymous reviewers wrote stimulating, thorough, and fair
reviews. This work was triggered by discussions with Oded Aharonson,
Jeff Andrews-Hanna, and Devon Burr. Discussions with Mark Allen,
Konstantin Batygin, Bill Cassata, Bill Dietrich, Bethany Ehlmann, John
Eiler, Woody Fischer, John Grotzinger, Alex Hayes, Jim Head, Joel
Hurowitz, Ross Irwin, Gary Kocurek, Misha Kreslavsky, Mike Lamb, Vedran
Lekic, Alejandro Soto, Ken Tanaka, Aaron Wolf and Robin Wordsworth
supplied us with new ideas and refined our existing ones. E.S.K. is
grateful to Oded Aharonson, Woody Fischer, Francois Forget, John
Grotzinger, Kevin Lewis, Joannah Metz, Mikki Osterloo, Robin Wordsworth,
and James Wray for sharing their preprints and datasets. This research
was supported by the U.S. taxpayer through NASA Grants NNX08AN13G,
NNX09AN18G, and NNX09AL20G (to M.M.), NNX11AF51G (to Oded Aharonson),
and NSF Teragrid allocation TG-EAR100023. I.H. acknowledges support from
a Sir Charles Clore Prize for Outstanding Appointment in the
Experimental Sciences at the Weizmann Institute of Science, and an Alon
Fellowship for Young P.I.s from the Israeli Committee for Higher
Education. E.S.K. is supported at Caltech by an O.K. Earl Fellowship.
NR 278
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PI SAN DIEGO
PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA
SN 0019-1035
EI 1090-2643
J9 ICARUS
JI Icarus
PD MAR
PY 2013
VL 223
IS 1
BP 181
EP 210
DI 10.1016/j.icarus.2012.11.034
PG 30
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 104FP
UT WOS:000315977600015
ER
PT J
AU Radeva, YL
Mumma, MJ
Villanueva, GL
Bonev, BP
DiSanti, MA
A'Hearn, MF
Dello Russo, N
AF Radeva, Yana L.
Mumma, Michael J.
Villanueva, Geronimo L.
Bonev, Boncho P.
DiSanti, Michael A.
A'Hearn, Michael F.
Dello Russo, Neil
TI High-resolution infrared spectroscopic measurements of Comet 2P/Encke:
Unusual organic composition and low rotational temperatures
SO ICARUS
LA English
DT Article
DE Comets, Composition; Infrared observations; Origin, Solar System;
Spectroscopy
ID GIOTTO SPACECRAFT ENCOUNTER; MONTE-CARLO-SIMULATION; VOLATILE
COMPOSITION; 103P/HARTLEY 2; ATMOSPHERES APPLICATION; PARENT VOLATILES;
CARBON-MONOXIDE; SOLAR-SYSTEM; WATER; JUPITER
AB We present high-resolution infrared spectroscopic measurements of the ecliptic Comet 2P/Encke, observed on 4-6 November 2003 during its close approach to the Earth, using the Near Infrared Echelle Spectrograph on the Keck II telescope. We present flux-calibrated spectra, production rates, and mixing ratios for H2O, CH3OH, HCN, H2CO, C2H2, C2H6, CH4 and CO. Comet 2P/Encke is a dynamical end-member among comets because of its short period of 3.3 years. Relative to "organics-normal" comets, we determined that 2P/Encke is depleted in HCN, H2CO, C2H2, C2H6, CH4 and CO, but it is enriched in CH3OH. We compared mixing ratios of these organic species measured on separate dates, and we see no evidence of macroscopic chemical heterogeneity in the nucleus of 2P/Encke, however, this conclusion is limited by sparse temporal sampling. The depleted abundances of most measured species suggest that 2P/Encke may have formed closer to the young Sun, before its insertion to the Kuiper belt, compared with "organics-normal" comets - as was previously suggested for other depleted comets (e.g. C/1999 S4 (LINEAR)). We measured very low rotational temperatures of 20-30 K for H2O, CH3OH and HCN in the near nucleus region of 2P/Encke, which correlate with one of the lowest cometary gas production rates (similar to 2.6 x 10(27) - molecules s(-1)) measured thus far in the infrared. This suggests that we are seeing the effects of more efficient radiative cooling, insufficient collisional excitation, and/or inefficient heating by fast H-atoms (and icy grains) in the observed region of the coma. Its extremely short orbital period, very low gas production rate, and classification as an ecliptic comet, make 2P/Encke an important addition to our growing database, and contribute significantly to the establishment of a chemical taxonomy of comets. (C) 2012 Elsevier Inc. All rights reserved.
C1 [Radeva, Yana L.; Villanueva, Geronimo L.; Bonev, Boncho P.] Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA.
[Radeva, Yana L.; Mumma, Michael J.; Villanueva, Geronimo L.; Bonev, Boncho P.; DiSanti, Michael A.] NASA, Goddard Ctr Astrobiol, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[A'Hearn, Michael F.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Dello Russo, Neil] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA.
RP Radeva, YL (reprint author), NASA, Goddard Space Flight Ctr, Mailstop 690-3, Greenbelt, MD 20771 USA.
EM yanaradeva@gmail.com
RI mumma, michael/I-2764-2013; Dello Russo, Neil/G-2727-2015
OI Dello Russo, Neil/0000-0002-8379-7304
FU NASA [RTOP 344-32-07, NNX08AW44A]; Astrobiology Institute [RTOP
344-53-51]; NASA's Planetary Astronomy [08-PAST08-0034, 09-PAST09-0034];
Planetary Atmospheres [08-PATM08-0031, 09-PATM09-0080]; NSF [1211362,
0807939]
FX This work was begun as part of YLR's Ph.D. dissertation at the
University of Maryland, College Park, under the supervision of MJM and
MFA. NASA supported YLR's Ph.D. research under the Planetary Astronomy
Program (RTOP 344-32-07 to M.J.M.), and the Astrobiology Institute (RTOP
344-53-51 to MJM). G.L.V. and M.A.D. acknowledge support from NASA's
Planetary Astronomy (08-PAST08-0034 to G.L.V., 09-PAST09-0034 to M.A.D.)
and Planetary Atmospheres (08-PATM08-0031 to G.L.V., 09-PATM09-0080 to
M.A.D.) Programs. BPB acknowledges support by NSF's Astronomy and
Astrophysics Research Grants Program NSF (1211362; 0807939) and by
Cooperative Agreement NASA#NNX08AW44A. We thank Hideyo Kawakita and
Reiko Furusho for their helpful feedback in preparing the observations.
The data presented herein were obtained at the W.M. Keck Observatory,
operated as a scientific partnership among CalTech, UCLA, and NASA. This
Observatory was made possible by the generous financial support of the
W.M. Keck Foundation.
NR 65
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PI SAN DIEGO
PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA
SN 0019-1035
J9 ICARUS
JI Icarus
PD MAR
PY 2013
VL 223
IS 1
BP 298
EP 307
DI 10.1016/j.icarus.2012.11.023
PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 104FP
UT WOS:000315977600021
ER
PT J
AU Pifko, S
Janches, D
Close, S
Sparks, J
Nakamura, T
Nesvorny, D
AF Pifko, Steven
Janches, Diego
Close, Sigrid
Sparks, Jonathan
Nakamura, Takuji
Nesvorny, David
TI The Meteoroid Input Function and predictions of mid-latitude meteor
observations by the MU radar
SO ICARUS
LA English
DT Article
DE Meteors; Radar observations; Instrumentation
ID LARGE-APERTURE RADARS; HEAD ECHO DATA; 430 MHZ RADAR; VELOCITY
DISTRIBUTION; HIGH-POWER; HIGH-RESOLUTION; ARECIBO; DISTRIBUTIONS; MASS;
SCATTERING
AB The majority of extraterrestrial particles entering Earth's atmosphere originate from the Sporadic Meteoroid Complex (SMC) and are associated with many mesospheric layer phenomena. The Meteoroid Input Function (MIF) is a model that has been developed with the purpose of understanding the temporal and spatial variability of the meteoroid impact in the atmosphere. The MIF has been shown to accurately predict the seasonal and diurnal variations of the meteor flux observed by High Power Large Aperture (HPLA) radars at various geographic locations, including the Arecibo Observatory (AO) and the Poker Flat Incoherent Scatter Radar (PFISR). For this, the model requires the assessment of a potential observational bias of the particular HPLA radar utilized: the minimum detectable radar cross-section (RCS). The RCS sensitivity threshold provides a metric to characterize the radar system's ability to detect particles with a given mass and speed. In this paper, the MIF model was used to predict meteor properties (e.g. the distributions of areal density, speed, and radiant location) observed by the Middle and Upper atmosphere (MU) radar while leveraging the system's interferometric capability to address the model's ability to predict meteor observations at middle geographic latitudes and for a radar operating frequency in the low VHF band. This study demonstrates that the MIF accurately considered the speed and sporadic source distributions for the portion of the meteoroid population observable by the MU radar, and the applicability of the MIF to the MU system increases the confidence of using it as a global model. (C) 2013 Elsevier Inc. All rights reserved.
C1 [Pifko, Steven; Close, Sigrid] Stanford Univ, Dept Aeronaut & Astronaut, Space Environm & Satellite Syst Lab, Palo Alto, CA 94305 USA.
[Janches, Diego] NASA, Space Weather Lab, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Sparks, Jonathan] Univ Washington, Dept Phys, Seattle, WA 98105 USA.
[Nakamura, Takuji] Natl Inst Polar Res, Tokyo, Japan.
[Nesvorny, David] SW Res Inst, Boulder, CO 80302 USA.
RP Pifko, S (reprint author), Stanford Univ, Dept Aeronaut & Astronaut, Space Environm & Satellite Syst Lab, Palo Alto, CA 94305 USA.
EM spifko@stanford.edu
RI Janches, Diego/D-4674-2012
OI Janches, Diego/0000-0001-8615-5166
FU NSF [AST-0908118, AGS-0525655]; Japanese Society for the Promotion of
Science (JSPS)
FX The MU radar system belongs to and is operated by the Research Institute
of Sustainable Humanosphere (RISH), Kyoto University, Uji, Kyoto, Japan.
S.P., D.J., and J.J.S. were supported under NSF Grants AST-0908118 and
AGS-0525655 to NorthWest Research Associates, Inc. D.J. is grateful to
the Japanese Society for the Promotion of Science (JSPS) who supported
his visit to the University of Kyoto, Japan, in 2009 under a short term
fellowship, making the observations presented here and this study
possible.
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PI SAN DIEGO
PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA
SN 0019-1035
J9 ICARUS
JI Icarus
PD MAR
PY 2013
VL 223
IS 1
BP 444
EP 459
DI 10.1016/j.icarus.2012.12.014
PG 16
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 104FP
UT WOS:000315977600032
ER
PT J
AU Sayanagi, KM
Dyudina, UA
Ewald, SP
Fischer, G
Ingersoll, AP
Kurth, WS
Muro, GD
Porco, CC
West, RA
AF Sayanagi, Kunio M.
Dyudina, Ulyana A.
Ewald, Shawn P.
Fischer, Georg
Ingersoll, Andrew P.
Kurth, William S.
Muro, Gabriel D.
Porco, Carolyn C.
West, Robert A.
TI Dynamics of Saturn's great storm of 2010-2011 from Cassini ISS and RPWS
SO ICARUS
LA English
DT Article
DE Saturn, Atmosphere; Atmospheres, Dynamics; Meteorology
ID 1990 EQUATORIAL DISTURBANCE; RED SPOT; CLOUD FEATURES; JOVIAN
ATMOSPHERES; IMAGING SCIENCE; ZONAL WINDS; WHITE SPOT; JUPITERS; IMAGES;
EVOLUTION
AB Saturn's quasi-periodic planet-encircling storms are the largest convecting cumulus outbursts in the Solar System. The last eruption was in 1990 (Sanchez-Lavega, A. [1994]. Chaos 4, 341-353). A new eruption started in December 2010 and presented the first-ever opportunity to observe such episodic storms from a spacecraft in orbit around Saturn (Fischer, G. et al. [2011]. Nature 475, 75-77; Sanchez-Lavega, A. et al. [2011]. Nature 475,71-74; Fletcher, L.N. et al. [2011]. Science 332, 1413). Here, we analyze images acquired with the Cassini Imaging Science Subsystem (ISS), which captured the storm's birth, evolution, and demise. In studying the end of the convective activity, we also analyze the Saturn Electrostatic Discharge (SED) signals detected by the Radio and Plasma Wave Science (RPWS) instrument. The storm's initial position coincided with that of a previously known feature called the String of Pearls (SoPs) at 33 degrees N planetocentric latitude. Intense cumulus convection at the westernmost point of the storm formed a particularly bright "head" that drifted at -26.9 +/- 0.8 m s(-1) (negative denotes westward motion). On January 11, 2011, the size of the head was 9200 km and up to 34,000 km in the north-south and east-west dimensions, respectively. RPWS measurements show that the longitudinal extent of the lightning source expanded with the storm's growth. The storm spawned the largest tropospheric vortex ever seen on Saturn. On January 11, 2011, the anticyclone was sized 11,000 km by 12,000 km in the north-south and east-west directions, respectively. Between January and September 2011, the vortex drifted at an average speed of -8.4 m s(-1). We detect anticyclonic circulation in the new vortex. The vortex's size gradually decreased after its formation, and its central latitude shifted to the north. The storm's head moved westward and encountered the new anticyclone from the east in June 2011. After the head-vortex collision, the RPWS instrument detected that the SED activities became intermittent and declined over similar to 40 days until the signals became undetectable in early August. In late August, the SED radio signals resurged for 9 days. The storm left a vast dark area between 32 degrees N and 38 degrees N latitudes, surrounded by a highly disturbed region that resembles the mid-latitudes of Jupiter. Using ISS images, we also made cloud-tracking wind measurements that reveal differences in the cloud-level zonal wind profiles before and after the storm. (C) 2012 Elsevier Inc. All rights reserved.
C1 [Sayanagi, Kunio M.] Hampton Univ, Dept Atmospher & Planetary Sci, Hampton, VA 23668 USA.
[Sayanagi, Kunio M.; Dyudina, Ulyana A.; Ewald, Shawn P.; Ingersoll, Andrew P.; Muro, Gabriel D.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA.
[Fischer, Georg] Austrian Acad Sci, Space Res Inst, A-8042 Graz, Austria.
[Fischer, Georg; Kurth, William S.] Univ Iowa, Dept Phys & Astron, Iowa City, IA 52242 USA.
[Muro, Gabriel D.] Univ Calif Santa Cruz, Dept Earth & Planetary Sci, Santa Cruz, CA 95064 USA.
[Porco, Carolyn C.] Space Sci Inst, Cassini Imaging Cent Lab Operat, Boulder, CO 80301 USA.
[West, Robert A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Sayanagi, KM (reprint author), Hampton Univ, Dept Atmospher & Planetary Sci, Hampton, VA 23668 USA.
EM kunio.sayanagi@hamptonu.edu
OI Kurth, William/0000-0002-5471-6202
FU Cassini-Huygens mission; NASA; ESA; ASI; Austrian Science Fund (FWF)
[P24325-N16]; University of Iowa
FX Our work was supported by the Cassini-Huygens mission, a cooperative
project of NASA, ESA, ASI, managed by JPL, a division of the California
Institute of Technology, under a contract with NASA. The authors thank
the two anonymous reviewers for their very constructive comments. G.F.
was supported by a grant from the Austrian Science Fund (FWF project
P24325-N16) and by a short-term scholarship at the University of Iowa.
NR 69
TC 35
Z9 35
U1 2
U2 20
PU ACADEMIC PRESS INC ELSEVIER SCIENCE
PI SAN DIEGO
PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA
SN 0019-1035
EI 1090-2643
J9 ICARUS
JI Icarus
PD MAR
PY 2013
VL 223
IS 1
BP 460
EP 478
DI 10.1016/j.icarus.2012.12.013
PG 19
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 104FP
UT WOS:000315977600033
ER
PT J
AU McGovern, JA
Bussey, DB
Greenhagen, BT
Paige, DA
Cahill, JTS
Spudis, PD
AF McGovern, J. Andrew
Bussey, D. Benjamin
Greenhagen, Benjamin T.
Paige, David A.
Cahill, Joshua T. S.
Spudis, Paul D.
TI Mapping and characterization of non-polar permanent shadows on the lunar
surface
SO ICARUS
LA English
DT Article
DE Moon, Surface; Solar radiation
ID WATER ICE; MOON; POLES; ILLUMINATION; DEPOSITS; MISSION
AB We present the first globally complete inventory of permanent shadows on the lunar surface that are detectable with the current global instrument datasets, including discovery of regions with persistent shadows over geologic time periods as close to the equator as +/- 58 degrees of latitude. These results were obtained through application of a ray tracing technique to the latest global topographic datasets from the Lunar Reconnaissance Orbiter. Our analysis reveals that 13,361 km(2) of surface in the northern hemisphere and 17,698 km(2) in the southern hemisphere are permanently shadowed. We present maps showing the locations of all the permanent shadows detectable using these datasets then turn our focus toward the permanent shadows farthest from the poles. Each permanent shadow on the equator side of +/- 65 degrees of latitude is shown in detail. Surface brightness temperature data derived from the Diviner mid-infrared radiometer on board the Lunar Reconnaissance Orbiter have been analyzed for four of these locations and found to have mid-day temperatures 75-120 K less than nearby comparison locations that experience direct daytime illumination. In some cases the permanently shadowed locations have night-time temperatures 10-25 K lower than surroundings. The temperature results support our finding that these non-polar craters are permanently shadowed. The surface brightness temperature results also raise interesting questions about their ability to cold trap volatiles. Discovery of these non-polar permanently shadowed regions increases possible locations of water resources and high priority exploration targets on the Moon. (C) 2013 Elsevier Inc. All rights reserved.
C1 [McGovern, J. Andrew; Bussey, D. Benjamin; Cahill, Joshua T. S.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA.
[Greenhagen, Benjamin T.] Jet Prop Lab, Pasadena, CA 91011 USA.
[Paige, David A.] Univ Calif Los Angeles, Los Angeles, CA 90095 USA.
[Spudis, Paul D.] Lunar & Planetary Inst, Houston, TX 77058 USA.
RP McGovern, JA (reprint author), Johns Hopkins Univ, Appl Phys Lab, Johns Hopkins Rd, Laurel, MD 20723 USA.
EM Andy.McGovern@jhuapl.edu
RI Cahill, Joshua/I-3656-2012; Greenhagen, Benjamin/C-3760-2016; Bussey,
Ben/D-7892-2016
OI Cahill, Joshua/0000-0001-6874-5533;
NR 29
TC 14
Z9 14
U1 0
U2 14
PU ACADEMIC PRESS INC ELSEVIER SCIENCE
PI SAN DIEGO
PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA
SN 0019-1035
J9 ICARUS
JI Icarus
PD MAR
PY 2013
VL 223
IS 1
BP 566
EP 581
DI 10.1016/j.icarus.2012.10.018
PG 16
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 104FP
UT WOS:000315977600039
ER
PT J
AU Haberle, RM
AF Haberle, Robert M.
TI Estimating the power of Mars' greenhouse effect
SO ICARUS
LA English
DT Article
DE Mars; Greenhouse effect; Effective temperature
AB Extensive modeling of Mars in conjunction with in situ observations suggests that the annual average global mean surface temperature is [(T) over bar (s)] similar to 202 K. Yet its effective temperature, i.e., the temperature at which a blackbody radiates away the energy it absorbs, is T-e similar to 208 K. How can a planet with a CO2 atmosphere have a mean annual surface temperature that is actually less than its effective temperature? We use the Ames General Circulation Model explain why this is the case and point out that the correct comparison of the effective temperature is with the effective surface temperature T-se, which is the fourth root of the annual and globally averaged value of T-s(4). This may seem obvious, but the distinction is often not recognized in the literature. Published by Elsevier Inc.
C1 NASA, Space Sci & Astrobiol Div, Ames Res Ctr, Moffett Field, CA 94035 USA.
RP Haberle, RM (reprint author), NASA, Space Sci & Astrobiol Div, Ames Res Ctr, MS 245-3, Moffett Field, CA 94035 USA.
EM Robert.M.Haberle@nasa.gov
FU NASA's Planetary Exploration Program
FX We thank NASA's Planetary Exploration Program for supporting this work,
and James Schaeffer for running, archiving, and extracting data from the
model to carry out the analysis.
NR 3
TC 2
Z9 2
U1 0
U2 9
PU ACADEMIC PRESS INC ELSEVIER SCIENCE
PI SAN DIEGO
PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA
SN 0019-1035
J9 ICARUS
JI Icarus
PD MAR
PY 2013
VL 223
IS 1
BP 619
EP 620
DI 10.1016/j.icarus.2012.12.022
PG 2
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 104FP
UT WOS:000315977600045
ER
PT J
AU Reddy, V
Le Corre, L
O'Brien, DP
Nathues, A
Cloutis, EA
Durda, DD
Bottke, WF
Bhatt, MU
Nesvorny, D
Buczkowski, D
Scully, JEC
Palmer, EM
Sierks, H
Mann, PJ
Becker, KJ
Beck, AW
Mittlefehldt, D
Li, JY
Gaskell, R
Russell, CT
Gaffey, MJ
McSween, HY
McCord, TB
Combe, JP
Blewett, D
AF Reddy, Vishnu
Le Corre, Lucille
O'Brien, David P.
Nathues, Andreas
Cloutis, Edward A.
Durda, Daniel D.
Bottke, William F.
Bhatt, Megha U.
Nesvorny, David
Buczkowski, Debra
Scully, Jennifer E. C.
Palmer, Elizabeth M.
Sierks, Holger
Mann, Paul J.
Becker, Kris J.
Beck, Andrew W.
Mittlefehldt, David
Li, Jian-Yang
Gaskell, Robert
Russell, Christopher T.
Gaffey, Michael J.
McSween, Harry Y.
McCord, Thomas B.
Combe, Jean-Philippe
Blewett, David
TI Delivery of dark material to Vesta via carbonaceous chondritic impacts
(vol 221, pg 544, 2012)
SO ICARUS
LA English
DT Correction
C1 [Reddy, Vishnu; Le Corre, Lucille; Nathues, Andreas; Bhatt, Megha U.; Sierks, Holger] Max Planck Inst Solar Syst Res, D-37191 Katlenburg Lindau, Germany.
[Reddy, Vishnu; Gaffey, Michael J.] Univ N Dakota, Dept Space Studies, Grand Forks, ND 58201 USA.
[O'Brien, David P.; Gaskell, Robert] Planetary Sci Inst, Tucson, AZ USA.
[Cloutis, Edward A.; Mann, Paul J.] Univ Winnipeg, Dept Geog, Winnipeg, MB R3B 2E9, Canada.
[Durda, Daniel D.; Bottke, William F.; Nesvorny, David] SW Res Inst, Boulder, CO USA.
[Buczkowski, Debra; Blewett, David] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD USA.
[Scully, Jennifer E. C.; Palmer, Elizabeth M.; Russell, Christopher T.] Univ Calif Los Angeles, Inst Geophys & Planetary Phys, Los Angeles, CA 90024 USA.
[Becker, Kris J.] US Geol Survey, Astrogeol Sci Ctr, Flagstaff, AZ 86001 USA.
[Beck, Andrew W.] Smithsonian Natl Museum Nat Hist, Dept Mineral Sci, Washington, DC USA.
[Mittlefehldt, David] NASA, Astromat Res Off, Johnson Space Ctr, Houston, TX USA.
[Li, Jian-Yang] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[McSween, Harry Y.] Univ Tennessee, Dept Earth & Planetary Sci, Knoxville, TN USA.
[McCord, Thomas B.; Combe, Jean-Philippe] Bear Fight Inst, Winthrop, WA USA.
RP Reddy, V (reprint author), Max Planck Inst Solar Syst Res, D-37191 Katlenburg Lindau, Germany.
EM reddy@mps.mpg.de
RI Blewett, David/I-4904-2012; Beck, Andrew/J-7215-2015
OI Blewett, David/0000-0002-9241-6358; Beck, Andrew/0000-0003-4455-2299
NR 1
TC 0
Z9 0
U1 1
U2 4
PU ACADEMIC PRESS INC ELSEVIER SCIENCE
PI SAN DIEGO
PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA
SN 0019-1035
J9 ICARUS
JI Icarus
PD MAR
PY 2013
VL 223
IS 1
BP 632
EP 632
DI 10.1016/j.icarus.2012.10.006
PG 1
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 104FP
UT WOS:000315977600049
ER
PT J
AU Akgiray, A
Weinreb, S
Imbriale, WA
Beaudoin, C
AF Akgiray, Ahmed
Weinreb, Sander
Imbriale, William A.
Beaudoin, Christopher
TI Circular Quadruple-Ridged Flared Horn Achieving Near-Constant Beamwidth
Over Multioctave Bandwidth: Design and Measurements
SO IEEE TRANSACTIONS ON ANTENNAS AND PROPAGATION
LA English
DT Article
DE Aperture antennas; horn antennas; radio astronomy; reflector antenna
feeds; reflector antennas; ridge waveguides; ultrawideband antennas
ID WAVE-GUIDES; ANTENNAS
AB A circular quadruple-ridged flared horn achieving almost-constant beamwidth over 6:1 bandwidth is presented. This horn is the first demonstration of a wideband feed for radio telescopes which is capable of accommodating different reflector antenna optics, maintains almost constant gain and has excellent match. Measurements of stand-alone horn performance reveal excellent return loss performance as well as stable radiation patterns over 6:1 frequency range. Physical optics calculations predict an average of 69% aperture efficiency and 13 K antenna noise temperature with the horn installed on a radio telescope.
C1 [Akgiray, Ahmed; Weinreb, Sander] CALTECH, Dept Elect Engn, Pasadena, CA 91125 USA.
[Imbriale, William A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Beaudoin, Christopher] MIT, Haystack Observ, Westford, MA 01886 USA.
RP Akgiray, A (reprint author), CALTECH, Dept Elect Engn, Pasadena, CA 91125 USA.
EM ahmed@caltech.edu; sweinreb@caltech.edu; imbriale@jpl.nasa.gov;
cbeaudoin@haystack.mit.edu
FU NSF through Cornell University [AST-0431486]; National Aeronautics and
Space Administration
FX Manuscript received January 21, 2012; revised June 02, 2012; accepted
November 09, 2012. Date of publication November 27, 2012; date of
current version February 27, 2013. This work was supported in part by
NSF Grant AST-0431486 through Cornell University for the SKA Technical
Development Program. Part of this research was carried out at the Jet
Propulsion Laboratory, California Institute of Technology, Pasadena, CA,
USA, under a contract with the National Aeronautics and Space
Administration.
NR 33
TC 21
Z9 22
U1 0
U2 4
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 0018-926X
J9 IEEE T ANTENN PROPAG
JI IEEE Trans. Antennas Propag.
PD MAR
PY 2013
VL 61
IS 3
BP 1099
EP 1108
DI 10.1109/TAP.2012.2229953
PG 10
WC Engineering, Electrical & Electronic; Telecommunications
SC Engineering; Telecommunications
GA 103ZM
UT WOS:000315958300011
ER
PT J
AU Ponchak, GE
AF Ponchak, George E.
TI Editorial: 2012 Radio Frequency Integrated Circuits (RFIC) Symposium
SO IEEE TRANSACTIONS ON MICROWAVE THEORY AND TECHNIQUES
LA English
DT Editorial Material
C1 NASA, Glenn Res Ctr, Cleveland, OH 44135 USA.
RP Ponchak, GE (reprint author), NASA, Glenn Res Ctr, Cleveland, OH 44135 USA.
NR 0
TC 0
Z9 0
U1 1
U2 3
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 0018-9480
J9 IEEE T MICROW THEORY
JI IEEE Trans. Microw. Theory Tech.
PD MAR
PY 2013
VL 61
IS 3
SI SI
BP 1005
EP 1005
DI 10.1109/TMTT.2013.2244371
PG 1
WC Engineering, Electrical & Electronic
SC Engineering
GA 104AM
UT WOS:000315961300001
ER
PT J
AU Foster, JE
Adamovsky, G
Gucker, SN
Blankson, IM
AF Foster, John E.
Adamovsky, Grigory
Gucker, Sarah Nowak
Blankson, Isaiah M.
TI A Comparative Study of the Time-Resolved Decomposition of Methylene Blue
Dye Under the Action of a Nanosecond Repetitively Pulsed DBD Plasma Jet
Using Liquid Chromatography and Spectrophotometry
SO IEEE TRANSACTIONS ON PLASMA SCIENCE
LA English
DT Article
DE Absorption; nonequilibrium; plasmas; pulsed power; water
ID ADVANCED OXIDATION PROCESSES; WASTE-WATER; ELECTRICAL DISCHARGES; CORONA
DISCHARGE; AQUEOUS-SOLUTION; REMOVAL; ADSORPTION; PH; PHARMACEUTICALS;
PURIFICATION
AB An underwater dielectric barrier discharge (DBD) plasma jet excited by a repetitively pulsed nanosecond pulsed power modulator was used to study plasma-induced decolorization of a 1.4 x 10(-4) M solution of methylene blue (MB). Past plasma decolorization studies have focused on spectrophotometry as the main diagnostic to assess decomposition. Because spectrophotometry is a measure of changes in the structure of molecular color, it is not an absolute measure of decomposition. In this paper, high-pressure liquid chromatography is used in parallel with spectrophotometry for comparison purposes and to assess the degree of true decomposition. Spectrophotometry results were found to be in agreement with chromatography measurements, suggesting that, at least in the case of MB, spectrophotometry is an adequate measure of decomposition. Additionally, the utility of a dual plasma jet applicator for rapid contaminant decomposition was explored.
C1 [Foster, John E.; Gucker, Sarah Nowak] Univ Michigan, Dept Nucl Engn, Ann Arbor, MI 48109 USA.
[Adamovsky, Grigory; Blankson, Isaiah M.] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA.
RP Foster, JE (reprint author), Univ Michigan, Dept Nucl Engn, Ann Arbor, MI 48109 USA.
FU NASA Faculty Fellowship Program (NASA Glenn); National Science
Foundation [CBET 1033141]
FX The authors would like to thank the NASA Faculty Fellowship Program
(NASA Glenn) and the National Science Foundation CBET 1033141 for
funding this research.
NR 38
TC 7
Z9 7
U1 3
U2 28
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 0093-3813
EI 1939-9375
J9 IEEE T PLASMA SCI
JI IEEE Trans. Plasma Sci.
PD MAR
PY 2013
VL 41
IS 3
BP 503
EP 512
DI 10.1109/TPS.2013.2245426
PG 10
WC Physics, Fluids & Plasmas
SC Physics
GA 107HD
UT WOS:000316205200014
ER
PT J
AU Wang, CX
Yang, P
Platnick, S
Heidinger, AK
Baum, BA
Greenwald, T
Zhang, ZB
Holz, RE
AF Wang, Chenxi
Yang, Ping
Platnick, Steven
Heidinger, Andrew K.
Baum, Bryan A.
Greenwald, Thomas
Zhang, Zhibo
Holz, Robert E.
TI Retrieval of Ice Cloud Properties from AIRS and MODIS Observations Based
on a Fast High-Spectral-Resolution Radiative Transfer Model
SO JOURNAL OF APPLIED METEOROLOGY AND CLIMATOLOGY
LA English
DT Article
ID BULK SCATTERING PROPERTIES; MULTIPLE-SCATTERING; OPTICAL-THICKNESS;
INFRARED-SPECTRA; CIRRUS CLOUD; PART I; TROPICAL CIRRUS; DOUBLING
METHOD; ATMOSPHERES; ABSORPTION
AB A computationally efficient high-spectral-resolution cloudy-sky radiative transfer model (HRTM) in the thermal infrared region (700-1300 cm(-1), 0.1 cm(-1) spectral resolution) is advanced for simulating the up-welling radiance at the top of atmosphere and for retrieving cloud properties. A precomputed transmittance database is generated for simulating the absorption contributed by up to seven major atmospheric absorptive gases (H2O, CO2, O-3, O-2, CH4, CO, and N2O) by using a rigorous line-by-line radiative transfer model (LBLRTM). Both the line absorption of individual gases and continuum absorption are included in the database. A high-spectral-resolution ice particle bulk scattering properties database is employed to simulate the radiation transfer within a vertically nonisothermal ice cloud layer. Inherent to HRTM are sensor spectral response functions that couple with high-spectral-resolution measurements in the thermal infrared regions from instruments such as the Atmospheric Infrared Sounder (AIRS) and Infrared Atmospheric Sounding Interferometer. When compared with the LBLRTM and the discrete ordinates radiative transfer model (DISORT), the root-mean-square error of HRTM-simulated single-layer cloud brightness temperatures in the thermal infrared window region is generally smaller than 0.2 K. An ice cloud optical property retrieval scheme is developed using collocated AIRS and Moderate Resolution Imaging Spectroradiometer (MODIS) data. A retrieval method is proposed to take advantage of the high-spectral-resolution instrument. On the basis of the forward model and retrieval method, a case study is presented for the simultaneous retrieval of ice cloud optical thickness tau and effective particle size D-eff that includes a cloud-top-altitude self-adjustment approach to improve consistency with simulations.
C1 [Wang, Chenxi; Yang, Ping] Texas A&M Univ, Dept Atmospher Sci, College Stn, TX 77843 USA.
[Platnick, Steven] NASA Goddard Space Flight Ctr, Div Earth Sci, Greenbelt, MD USA.
[Heidinger, Andrew K.] NOAA NESDIS Ctr Satellite Applicat & Res, Madison, WI USA.
[Baum, Bryan A.; Greenwald, Thomas; Holz, Robert E.] Univ Wisconsin, Space Sci & Engn Ctr, Madison, WI USA.
[Zhang, Zhibo] Univ Maryland Baltimore Cty, Baltimore, MD 21228 USA.
RP Wang, CX (reprint author), Texas A&M Univ, Dept Atmospher Sci, College Stn, TX 77843 USA.
EM chenx.wang@geos.tamu.edu
RI Yang, Ping/B-4590-2011; Baum, Bryan/B-7670-2011; Platnick,
Steven/J-9982-2014; Heidinger, Andrew/F-5591-2010; Zhang,
Zhibo/D-1710-2010
OI Baum, Bryan/0000-0002-7193-2767; Platnick, Steven/0000-0003-3964-3567;
Heidinger, Andrew/0000-0001-7631-109X; Zhang, Zhibo/0000-0001-9491-1654
FU NASA [NNX11AK37G, NNX11AF40G]; University of Wisconsin to Texas AM
University [301K630]
FX This study was partly supported by NASA Grant NNX11AK37G, for which the
principal investigator (PI) is Dr. Ping Yang; a subcontract (Contract
301K630) issued by the University of Wisconsin to Texas A&M University
associated with a NASA grant (NNX11AF40G), for which the PI is Dr. Bryan
Baum and the coinvestigators are Dr. Ping Yang and Dr. Andrew
Heymsfield; and the endowment funds related to the David Bullock Harris
Chair in Geosciences at the College of Geosciences, Texas A&M
University. The Texas A&M Supercomputing Facility (http://sc.tamu.edu/)
provides computational resources for the research reported in this
paper.
NR 58
TC 14
Z9 15
U1 0
U2 8
PU AMER METEOROLOGICAL SOC
PI BOSTON
PA 45 BEACON ST, BOSTON, MA 02108-3693 USA
SN 1558-8424
EI 1558-8432
J9 J APPL METEOROL CLIM
JI J. Appl. Meteorol. Climatol.
PD MAR
PY 2013
VL 52
IS 3
BP 710
EP 726
DI 10.1175/JAMC-D-12-020.1
PG 17
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 110ST
UT WOS:000316466700015
ER
PT J
AU Young, SA
Vaughan, MA
Kuehn, RE
Winker, DM
AF Young, Stuart A.
Vaughan, Mark A.
Kuehn, Ralph E.
Winker, David M.
TI The Retrieval of Profiles of Particulate Extinction from Cloud-Aerosol
Lidar and Infrared Pathfinder Satellite Observations (CALIPSO) Data:
Uncertainty and Error Sensitivity Analyses
SO JOURNAL OF ATMOSPHERIC AND OCEANIC TECHNOLOGY
LA English
DT Article
ID BACKSCATTER; ALGORITHM; PERFORMANCE; CALIBRATION; SIMULATION; RETURNS
AB Profiles of atmospheric cloud and aerosol extinction coefficients are retrieved on a global scale from measurements made by the lidar on board the Cloud-Aerosol Lidar and Infrared Pathfinder Satellite Observations (CALIPSO) mission since mid-June 2006. This paper presents an analysis of how the uncertainties in the inputs to the extinction retrieval algorithm propagate as the retrieval proceeds downward to lower levels of the atmosphere. The mathematical analyses, which are being used to calculate the uncertainties reported in the current (version 3) data release, are supported by figures illustrating the retrieval uncertainties in both simulated and actual data. Equations are also derived that describe the sensitivity of the extinction retrieval algorithm to errors in profile calibration and in the lidar ratios used in the retrievals. Biases that could potentially result from low signal-to-noise ratios in the data are also examined. Using simulated data, the propagation of bias errors resulting from errors in profile calibration and lidar ratios is illustrated.
C1 [Young, Stuart A.] CSIRO Marine & Atmospher Res, Aspendale, Vic 3195, Australia.
[Vaughan, Mark A.; Winker, David M.] NASA, Hampton, VA USA.
[Kuehn, Ralph E.] Univ Wisconsin, Space Sci & Engn Ctr, Madison, WI USA.
RP Young, SA (reprint author), CSIRO Marine & Atmospher Res, Private Bag 1, Aspendale, Vic 3195, Australia.
EM stuart.young@csiro.au
RI Young, Stuart/A-8641-2011
OI Young, Stuart/0000-0001-6434-9816
NR 31
TC 29
Z9 29
U1 0
U2 26
PU AMER METEOROLOGICAL SOC
PI BOSTON
PA 45 BEACON ST, BOSTON, MA 02108-3693 USA
SN 0739-0572
J9 J ATMOS OCEAN TECH
JI J. Atmos. Ocean. Technol.
PD MAR
PY 2013
VL 30
IS 3
BP 395
EP 428
DI 10.1175/JTECH-D-12-00046.1
PG 34
WC Engineering, Ocean; Meteorology & Atmospheric Sciences
SC Engineering; Meteorology & Atmospheric Sciences
GA 111YP
UT WOS:000316558500002
ER
PT J
AU Radkevich, A
Khlopenkov, K
Rutan, D
Kato, S
AF Radkevich, Alexander
Khlopenkov, Konstantin
Rutan, David
Kato, Seiji
TI A Supplementary Clear-Sky Snow and Ice Recognition Technique for CERES
Level 2 Products
SO JOURNAL OF ATMOSPHERIC AND OCEANIC TECHNOLOGY
LA English
DT Article
ID MODIS; CLOUDS; INVERSIONS; SATELLITE; TERRA
AB Identification of clear-sky snow and ice is an important step in the production of cryosphere radiation budget products, which are used in the derivation of long-term data series for climate research. In this paper, a new method of clear-sky snow/ice identification for Moderate Resolution Imaging Spectroradiometer (MODIS) is presented. The algorithm's goal is to enhance the identification of snow and ice within the Clouds and the Earth's Radiant Energy System (CERES) data after application of the standard CERES scene identification scheme. The input of the algorithm uses spectral radiances from five MODIS bands and surface skin temperature available in the CERES Single Scanner Footprint (SSF) product. The algorithm produces a cryosphere rating from an aggregated test: a higher rating corresponds to a more certain identification of the clear-sky snow/ice-covered scene. Empirical analysis of regions of interest representing distinctive targets such as snow, ice, ice and water clouds, open waters, and snow-free land selected from a number of MODIS images shows that the cryosphere rating of snow/ice targets falls into 95% confidence intervals lying above the same confidence intervals of all other targets. This enables recognition of clear-sky cryosphere by using a single threshold applied to the rating, which makes this technique different from traditional branching techniques based on multiple thresholds. Limited tests show that the established threshold clearly separates the cryosphere rating values computed for the cryosphere from those computed for noncryosphere scenes, whereas individual tests applied consequently cannot reliably identify the cryosphere for complex scenes.
C1 [Radkevich, Alexander; Khlopenkov, Konstantin; Rutan, David] SSAI, Hampton, VA 23666 USA.
[Kato, Seiji] NASA, Langley Res Ctr, Hampton, VA 23665 USA.
RP Radkevich, A (reprint author), SSAI, 1 Enterprise Pkwy, Hampton, VA 23666 USA.
EM alexander.radkevich@nasa.gov
NR 29
TC 1
Z9 1
U1 1
U2 7
PU AMER METEOROLOGICAL SOC
PI BOSTON
PA 45 BEACON ST, BOSTON, MA 02108-3693 USA
SN 0739-0572
J9 J ATMOS OCEAN TECH
JI J. Atmos. Ocean. Technol.
PD MAR
PY 2013
VL 30
IS 3
BP 557
EP 568
DI 10.1175/JTECH-D-12-00100.1
PG 12
WC Engineering, Ocean; Meteorology & Atmospheric Sciences
SC Engineering; Meteorology & Atmospheric Sciences
GA 111YP
UT WOS:000316558500011
ER
PT J
AU Takahashi, Y
Scheeres, DJ
Werner, RA
AF Takahashi, Yu
Scheeres, D. J.
Werner, Robert A.
TI Surface Gravity Fields for Asteroids and Comets
SO JOURNAL OF GUIDANCE CONTROL AND DYNAMICS
LA English
DT Article
ID SHAPE; EROS
AB The characteristics of the interior gravity field are derived, summarized, and evaluated near the surface of an asteroid for the purpose of small body proximity operations. In order to characterize the gravity field of a body, the exterior gravity field is widely in use. However, the exterior gravity field expression breaks down when computing the potential and its gradients within the Brillouin sphere, meaning that spacecraft dynamics cannot be modeled accurately in close proximity to the body's surface. On the other hand, the convergence of the potential and its gradients are guaranteed within the Brillouin sphere of the interior potential, a feature that enables the gravity field modeling near the surface of a body. After derivation, a technique for converting an exterior gravity field or a polyhedral gravity field into an interior gravity field is outlined, a method to numerically approximate the interior spherical harmonic coefficients for a body with a homogeneous density distribution is introduced, and comparisons between the spacecraft dynamics propagated in the polyhedral gravity field and the interior gravity field are made. The results show that the interior gravity field models the gravity field environment well in close proximity to the body's surface.
C1 [Takahashi, Yu; Scheeres, D. J.] Univ Colorado, Boulder, CO 80309 USA.
[Werner, Robert A.] CALTECH, Jet Prop Lab, Mission Design & Nav Sect, Pasadena, CA 91109 USA.
RP Takahashi, Y (reprint author), Univ Colorado, 429 UCB, Boulder, CO 80309 USA.
EM yu.takahashi@colorado.edu; scheeres@colorado.edu;
robert.a.werner@jpl.nasa.gov
FU OSIRIS-REx mission through the University of Arizona; Jet Propulsion
Laboratory
FX Y. Takahashi and D. J. Scheeres acknowledge funding from the OSIRIS-REx
mission through a grant from the University of Arizona. The authors
would like to acknowledge funding from the Jet Propulsion Laboratory and
thank Theodore Sweetser for his support of this research.
NR 26
TC 16
Z9 17
U1 3
U2 10
PU AMER INST AERONAUT ASTRONAUT
PI RESTON
PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA
SN 0731-5090
J9 J GUID CONTROL DYNAM
JI J. Guid. Control Dyn.
PD MAR-APR
PY 2013
VL 36
IS 2
BP 362
EP 374
DI 10.2514/1.59144
PG 13
WC Engineering, Aerospace; Instruments & Instrumentation
SC Engineering; Instruments & Instrumentation
GA 102GF
UT WOS:000315832200002
ER
PT J
AU Lee, HT
Meyn, LA
Kim, S
AF Lee, Hak-Tae
Meyn, Larry A.
Kim, SoYoung
TI Probabilistic Safety Assessment of Unmanned Aerial System Operations
SO JOURNAL OF GUIDANCE CONTROL AND DYNAMICS
LA English
DT Article
C1 [Lee, Hak-Tae; Kim, SoYoung] Univ Calif Santa Cruz, Moffett Field, CA 94035 USA.
[Meyn, Larry A.] NASA, Ames Res Ctr, Syst Modeling & Optimizat Branch, Moffett Field, CA 94035 USA.
RP Kim, S (reprint author), Sungkyunkwan Univ, Sch Informat & Commun Engn, Suwon 440746, South Korea.
NR 13
TC 4
Z9 4
U1 1
U2 4
PU AMER INST AERONAUT ASTRONAUT
PI RESTON
PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA
SN 0731-5090
J9 J GUID CONTROL DYNAM
JI J. Guid. Control Dyn.
PD MAR-APR
PY 2013
VL 36
IS 2
BP 610
EP 617
DI 10.2514/1.57572
PG 8
WC Engineering, Aerospace; Instruments & Instrumentation
SC Engineering; Instruments & Instrumentation
GA 102GF
UT WOS:000315832200022
ER
PT J
AU Richardson, IG
AF Richardson, Ian G.
TI ASTROPHYSICS An unexpected shock
SO NATURE PHYSICS
LA English
DT News Item
ID ACCELERATION; ELECTRONS
C1 [Richardson, Ian G.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Richardson, Ian G.] NASA, Astroparticle Phys Lab, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Richardson, IG (reprint author), Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
EM ian.g.richardson@nasa.gov
OI Richardson, Ian/0000-0002-3855-3634
NR 7
TC 0
Z9 0
U1 0
U2 4
PU NATURE PUBLISHING GROUP
PI LONDON
PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND
SN 1745-2473
J9 NAT PHYS
JI Nat. Phys.
PD MAR
PY 2013
VL 9
IS 3
BP 131
EP 132
PG 2
WC Physics, Multidisciplinary
SC Physics
GA 106PF
UT WOS:000316156300007
ER
PT J
AU Hauksson, E
Stock, J
Bilham, R
Boese, M
Chen, XW
Fielding, EJ
Galetzka, J
Hudnut, KW
Hutton, K
Jones, LM
Kanamori, H
Shearer, PM
Steidl, J
Treiman, J
Wei, SJ
Yang, WZ
AF Hauksson, Egill
Stock, Joann
Bilham, Roger
Boese, Maren
Chen, Xiaowei
Fielding, Eric J.
Galetzka, John
Hudnut, Kenneth W.
Hutton, Kate
Jones, Lucile M.
Kanamori, Hiroo
Shearer, Peter M.
Steidl, Jamie
Treiman, Jerry
Wei, Shengji
Yang, Wenzheng
TI Report on the August 2012 Brawley Earthquake Swarm in Imperial Valley,
Southern California
SO SEISMOLOGICAL RESEARCH LETTERS
LA English
DT Article
ID BAND REGIONAL SEISMOGRAMS; SALTON TROUGH; FOCAL MECHANISMS; NOVEMBER
1987; SAN-ANDREAS; FAULT; RUPTURE; INVERSION; ZIRCON
C1 [Hauksson, Egill; Stock, Joann; Boese, Maren; Galetzka, John; Hutton, Kate; Kanamori, Hiroo; Wei, Shengji; Yang, Wenzheng] CALTECH, Pasadena, CA 91125 USA.
[Bilham, Roger] Univ Colorado, Dept Geol Sci, Boulder, CO 80309 USA.
[Chen, Xiaowei; Shearer, Peter M.] Univ Calif San Diego, Inst Geophys & Planetary Phys 0225, La Jolla, CA 92093 USA.
[Fielding, Eric J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Hudnut, Kenneth W.; Jones, Lucile M.] US Geol Survey, Pasadena, CA 91106 USA.
[Steidl, Jamie] Univ Calif Santa Barbara, Earth Res Inst, Santa Barbara, CA 93106 USA.
[Treiman, Jerry] Calif Geol Survey, Los Angeles, CA 90017 USA.
RP Hauksson, E (reprint author), CALTECH, 1200 East Calif Blvd, Pasadena, CA 91125 USA.
EM hauksson@caltech.edu
RI Hudnut, Kenneth/B-1945-2009; Shearer, Peter/K-5247-2012; Wei,
Shengji/M-2137-2015; Fielding, Eric/A-1288-2007;
OI Hudnut, Kenneth/0000-0002-3168-4797; Shearer, Peter/0000-0002-2992-7630;
Wei, Shengji/0000-0002-0319-0714; Fielding, Eric/0000-0002-6648-8067;
Stock, Joann Miriam/0000-0003-4816-7865; Bilham,
Roger/0000-0002-5547-4102; Hauksson, Egill/0000-0002-6834-5051
FU National Earthquake Hazards Reduction Program/USGS [12HQPA0001];
Southern California Earthquake Center (SCEC); National Science
Foundation (NSF) [EAR-0529922, 07HQAG0008]; National Aeronautics and
Space Administration (NASA) Earth Surface and Interior focus area; NSF
[OCE-0742253]; Network for Earthquake Engineering Simulation program of
the NSF [CMMI-0927178]
FX We thank the personnel of the United States Geological Survey
(USGS)-California Institute of Technology (Caltech) Southern California
Seismic Network (SCSN) for picking the arrival times and archiving the
seismograms and the Southern California Earthquake Data Center for
distributing the data. TerraSAR-X data are copyright 2012 DLR and were
provided under the Group on Earth Observation (GEO) Geohazard Supersite
program project prlund_GEO0927. E. Hauksson and W. Yang were supported
by the National Earthquake Hazards Reduction Program/USGS Grant
12HQPA0001. This research was also supported by the Southern California
Earthquake Center (SCEC), which is funded by National Science Foundation
(NSF) Cooperative Agreement EAR-0529922 and USGS Cooperative Agreement
07HQAG0008. This paper is Contribution 1678 of SCEC and Contribution
10083 of the Division of Geological and Planetary Sciences, Caltech,
Pasadena, California.; We thank K. Marty (Imperial Valley College) and
S. Williams (consulting geologist from Imperial, California) for help
with fieldwork. The high-rate GPS data were processed and provided by S.
Owen from the Jet Propulsion Laboratory (JPL). Part of this research was
supported by the National Aeronautics and Space Administration (NASA)
Earth Surface and Interior focus area and performed at the JPL, Caltech.
We thank G. Fuis and D. Hill for reviews and J. Hole for valuable
discussions about the tectonics and velocity structure. J. Stock's
participation was supported by NSF Grant OCE-0742253.; The University of
California at Santa Barbara operates the Wildlife Liquefaction Array
facility, with funding through the George E. Brown, Jr., Network for
Earthquake Engineering Simulation program of the NSF under Award
CMMI-0927178. Most figures were done using GMT (Wessel and Smith, 1998).
NR 52
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PU SEISMOLOGICAL SOC AMER
PI ALBANY
PA 400 EVELYN AVE, SUITE 201, ALBANY, CA 94706-1375 USA
SN 0895-0695
EI 1938-2057
J9 SEISMOL RES LETT
JI Seismol. Res. Lett.
PD MAR-APR
PY 2013
VL 84
IS 2
BP 177
EP 189
DI 10.1785/0220120169
PG 13
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 101AP
UT WOS:000315747800003
ER
PT J
AU Sankararaman, S
MeLemore, K
Mahadevan, S
Bradford, SC
Peterson, LD
AF Sankararaman, Shankar
MeLemore, Kyle
Mahadevan, Sankaran
Bradford, Samuel Case
Peterson, Lee D.
TI Test Resource Allocation in Hierarchical Systems Using Bayesian Networks
SO AIAA JOURNAL
LA English
DT Article
ID RELIABILITY-ANALYSIS; POLYNOMIAL CHAOS; MODELS; VALIDATION; ALGORITHM;
MACHINE
AB This paper develops analytical methods for test resource allocation that aid in reducing the uncertainty in the system model prediction for multilevel and multidisciplinary systems. The various component, subsystem, and system-level model predictions; the corresponding inputs and calibration parameters; test data; and model and measurement errors are connected efficiently using a Bayesian network. This provides a unified framework for uncertainty analysis where test data can be integrated along with computational simulations. The Bayesian network is used in an inverse problem where the model parameters of multiple subsystems are calibrated simultaneously. This leads to a decrease in the variance of the model parameters, and hence, in the valiance of the overall system performance prediction. An optimization-based procedure is then used for test resource allocation using the Bayesian network, and those tests that can effectively reduce the uncertainty in the system model prediction are identified. The proposed methods are extended to three types of aerospace systems-testing applications: structural dynamics (multilevel), thermally induced vibration/flutter (multidisciplinary), and simplified space telescope mirror (multilevel, multidisciplinary).
C1 [Sankararaman, Shankar; MeLemore, Kyle; Mahadevan, Sankaran] Vanderbilt Univ, Dept Civil Engn, Nashville, TN 37235 USA.
[Bradford, Samuel Case; Peterson, Lee D.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Mahadevan, S (reprint author), Vanderbilt Univ, Dept Civil Engn, 221 Kirkland Hall, Nashville, TN 37235 USA.
EM shankar.sankararaman@gmail.com; kyle71788@gmail.com;
sankaran.mahadevan@vanderbilt.edu; Samuel.C.Bradford@jpl.nasa.gov;
Lee.D.Peterson@jpl.nasa.gov
OI Sankararaman, Shankar/0000-0002-6183-3562
FU National Aeronautics and Space Administration; Jet Propulsion
Laboratory, California Institute of Technology [RSA 1400821]
FX This study was performed at Vanderbilt University and the Jet Propulsion
Laboratory, California Institute of Technology, under contract no. RSA
1400821, funded by the National Aeronautics and Space Administration.
The computational resources of Vanderbilt University's Advanced
Computing Center for Research and Education (ACCRE) have been used for
the MATLAB simulations in this paper. The authors also appreciate
computational support by Chen Liang, graduate student at Vanderbilt
University.
NR 47
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PU AMER INST AERONAUT ASTRONAUT
PI RESTON
PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA
SN 0001-1452
J9 AIAA J
JI AIAA J.
PD MAR
PY 2013
VL 51
IS 3
BP 537
EP 550
DI 10.2514/1.J051542
PG 14
WC Engineering, Aerospace
SC Engineering
GA 098LQ
UT WOS:000315551200001
ER
PT J
AU Mace, GN
Kirkpatrick, JD
Cushing, MC
Gelino, CR
Griffith, RL
Skrutskie, MF
Marsh, KA
Wright, EL
Eisenhardt, PR
McLean, IS
Thompson, MA
Mix, K
Bailey, V
Beichman, CA
Bloom, JS
Burgasser, AJ
Fortney, JJ
Hinz, PM
Knox, RP
Lowrance, PJ
Marley, MS
Morley, CV
Rodigas, TJ
Saumon, D
Sheppard, SS
Stock, ND
AF Mace, Gregory N.
Kirkpatrick, J. Davy
Cushing, Michael C.
Gelino, Christopher R.
Griffith, Roger L.
Skrutskie, Michael F.
Marsh, Kenneth A.
Wright, Edward L.
Eisenhardt, Peter R.
McLean, Ian S.
Thompson, Maggie A.
Mix, Katholeen
Bailey, Vanessa
Beichman, Charles A.
Bloom, Joshua S.
Burgasser, Adam J.
Fortney, Jonathan J.
Hinz, Philip M.
Knox, Russell P.
Lowrance, Patrick J.
Marley, Mark S.
Morley, Caroline V.
Rodigas, Timothy J.
Saumon, Didier
Sheppard, Scott S.
Stock, Nathan D.
TI A STUDY OF THE DIVERSE T DWARF POPULATION REVEALED BY WISE
SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES
LA English
DT Article
DE binaries: general; brown dwarfs; galaxies: active; infrared: stars;
stars: low-mass
ID INFRARED-SURVEY-EXPLORER; COOL BROWN DWARF; COLLISION-INDUCED
ABSORPTION; SUBSTELLAR MASS FUNCTION; SPITZER-SPACE-TELESCOPE; ADAPTIVE
OPTICS SYSTEM; PROPER-MOTION SURVEY; KECK II TELESCOPE; WIDE-FIELD
CAMERA; SKY SURVEY
AB We report the discovery of 87 new T dwarfs uncovered with the Wide-field Infrared Survey Explorer (WISE) and 3 brown dwarfs with extremely red near-infrared colors that exhibit characteristics of both L and T dwarfs. Two of the new T dwarfs are likely binaries with L7 +/- 1 primaries and mid-type T secondaries. In addition, our follow-up program has confirmed 10 previously identified T dwarfs and 4 photometrically selected L and T dwarf candidates in the literature. This sample, along with the previous WISE discoveries, triples the number of known brown dwarfs with spectral types later than T5. Using the WISE All-Sky Source Catalog we present updated color-color and color-type diagrams for all the WISE-discovered T and Y dwarfs. Near-infrared spectra of the new discoveries are presented along with spectral classifications. To accommodate later T dwarfs we have modified the integrated flux method of determining spectral indices to instead use the median flux. Furthermore, a newly defined J-narrow index differentiates the early-type Y dwarfs from late-type T dwarfs based on the J-band continuum slope. The K/J indices for this expanded sample show that 32% of late-type T dwarfs have suppressed K-band flux and are blue relative to the spectral standards, while only 11% are redder than the standards. Comparison of the Y/J and K/J index to models suggests diverse atmospheric conditions and supports the possible re-emergence of clouds after the L/T transition. We also discuss peculiar brown dwarfs and candidates that were found not to be substellar, including two young stellar objects and two active galactic nuclei. The substantial increase in the number of known late-type T dwarfs provides a population that will be used to test models of cold atmospheres and star formation. The coolest WISE-discovered brown dwarfs are the closest of their type and will remain the only sample of their kind for many years to come.
C1 [Mace, Gregory N.; Wright, Edward L.; McLean, Ian S.] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA.
[Mace, Gregory N.; Kirkpatrick, J. Davy; Gelino, Christopher R.; Griffith, Roger L.; Mix, Katholeen; Beichman, Charles A.; Lowrance, Patrick J.] CALTECH, Infrared Proc & Anal Ctr, Pasadena, CA 91125 USA.
[Cushing, Michael C.] Univ Toledo, Dept Phys & Astron, Toledo, OH 43606 USA.
[Skrutskie, Michael F.] Univ Virginia, Dept Astron, Charlottesville, VA 22904 USA.
[Marsh, Kenneth A.] Cardiff Univ, Sch Phys & Astron, Cardiff CF24 3AA, S Glam, Wales.
[Eisenhardt, Peter R.] NASA, Jet Prop Lab, Pasadena, CA 91109 USA.
[Thompson, Maggie A.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA.
[Bailey, Vanessa; Hinz, Philip M.; Knox, Russell P.; Rodigas, Timothy J.; Stock, Nathan D.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA.
[Bloom, Joshua S.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA.
[Burgasser, Adam J.] Univ Calif San Diego, Dept Phys, San Diego, CA 92093 USA.
[Burgasser, Adam J.] MIT, Dept Phys, Cambridge, MA 02139 USA.
[Fortney, Jonathan J.; Morley, Caroline V.] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA.
[Marley, Mark S.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Saumon, Didier] Los Alamos Natl Lab, Los Alamos, NM 87545 USA.
[Sheppard, Scott S.] Carnegie Inst Sci, Dept Terr Magnetism, Washington, DC 20015 USA.
RP Mace, GN (reprint author), Univ Calif Los Angeles, Dept Phys & Astron, 430 Portola Plaza,Box 951547, Los Angeles, CA 90095 USA.
EM gmace@astro.ucla.edu
OI Fortney, Jonathan/0000-0002-9843-4354; Marley, Mark/0000-0002-5251-2943;
Rodigas, Timothy/0000-0002-7535-2997; Bailey,
Vanessa/0000-0002-5407-2806
NR 105
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U1 0
U2 10
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0067-0049
J9 ASTROPHYS J SUPPL S
JI Astrophys. J. Suppl. Ser.
PD MAR
PY 2013
VL 205
IS 1
AR 6
DI 10.1088/0067-0049/205/1/6
PG 49
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 100EC
UT WOS:000315677600006
ER
PT J
AU Purcell, CR
Hoare, MG
Cotton, WD
Lumsden, SL
Urquhart, JS
Chandler, C
Churchwell, EB
Diamond, P
Dougherty, SM
Fender, RP
Fuller, G
Garrington, ST
Gledhill, TM
Goldsmith, PF
Hindson, L
Jackson, JM
Kurtz, SE
Marti, J
Moore, TJT
Mundy, LG
Muxlow, TWB
Oudmaijer, RD
Pandian, JD
Paredes, JM
Shepherd, DS
Smethurst, S
Spencer, RE
Thompson, MA
Umana, G
Zijlstra, AA
AF Purcell, C. R.
Hoare, M. G.
Cotton, W. D.
Lumsden, S. L.
Urquhart, J. S.
Chandler, C.
Churchwell, E. B.
Diamond, P.
Dougherty, S. M.
Fender, R. P.
Fuller, G.
Garrington, S. T.
Gledhill, T. M.
Goldsmith, P. F.
Hindson, L.
Jackson, J. M.
Kurtz, S. E.
Marti, J.
Moore, T. J. T.
Mundy, L. G.
Muxlow, T. W. B.
Oudmaijer, R. D.
Pandian, J. D.
Paredes, J. M.
Shepherd, D. S.
Smethurst, S.
Spencer, R. E.
Thompson, M. A.
Umana, G.
Zijlstra, A. A.
TI THE COORDINATED RADIO AND INFRARED SURVEY FOR HIGH-MASS STAR FORMATION.
II. SOURCE CATALOG
SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES
LA English
DT Article
DE catalogs; H II regions; radio continuum: general; radio continuum: ISM;
surveys; techniques: image processing
ID GALACTIC PLANE SURVEY; RMS SURVEY; MU-M; CIRCULAR-POLARIZATION; FORMING
REGIONS; HII-REGIONS; SKY SURVEY; MILKY-WAY; GHZ; ULTRACOMPACT
AB The CORNISH project is the highest resolution radio continuum survey of the Galactic plane to date. It is the 5 GHz radio continuum part of a series of multi-wavelength surveys that focus on the northern GLIMPSE region (10 degrees < l < 65 degrees.), observed by the Spitzer satellite in the mid-infrared. Observations with the Very Large Array in B and BnA configurations have yielded a 1 ''.5 resolution Stokes I map with a root mean square noise level better than 0.4mJy beam-1. Here we describe the data-processing methods and data characteristics, and present a new, uniform catalog of compact radio emission. This includes an implementation of automatic deconvolution that provides much more reliable imaging than standard CLEANing. A rigorous investigation of the noise characteristics and reliability of source detection has been carried out. We show that the survey is optimized to detect emission on size scales up to 14 '' and for unresolved sources the catalog is more than 90% complete at a flux density of 3.9 mJy. We have detected 3062 sources above a 7s detection limit and present their ensemble properties. The catalog is highly reliable away from regions containing poorly sampled extended emission, which comprise less than 2% of the survey area. Imaging problems have been mitigated by down-weighting the shortest spacings and potential artifacts flagged via a rigorous manual inspection with reference to the Spitzer infrared data. We present images of the most common source types found: H II regions, planetary nebulae, and radio galaxies. The CORNISH data and catalog are available online at http://cornish.leeds.ac.uk.
C1 [Purcell, C. R.; Hoare, M. G.; Lumsden, S. L.; Urquhart, J. S.; Oudmaijer, R. D.] Univ Leeds, Sch Phys & Astron, Leeds LS2 9JT, W Yorkshire, England.
[Purcell, C. R.; Diamond, P.; Fuller, G.; Garrington, S. T.; Muxlow, T. W. B.; Smethurst, S.; Spencer, R. E.; Zijlstra, A. A.] Univ Manchester, Sch Phys & Astron, Jodrell Bank Ctr Astrophys, Manchester M13 9PL, Lancs, England.
[Purcell, C. R.] Univ Sydney, Sydney Inst Astron SiFA, Sydney, NSW 2006, Australia.
[Cotton, W. D.] Natl Radio Astron Observ, Charlottesville, VA 22903 USA.
[Urquhart, J. S.; Diamond, P.; Hindson, L.] CSIRO Astron & Space Sci, Epping, NSW 1710, Australia.
[Urquhart, J. S.] Max Planck Inst Radioastron, D-53121 Bonn, Germany.
[Chandler, C.; Shepherd, D. S.] Natl Radio Astron Observ, Array Operat Ctr, Socorro, NM 87801 USA.
[Churchwell, E. B.] Univ Wisconsin, Dept Astron, Madison, WI 53706 USA.
[Dougherty, S. M.] Natl Res Council Canada, Herzberg Inst Astrophys, Domin Radio Astrophys Observ, Penticton, BC V2A 6J9, Canada.
[Fender, R. P.] Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England.
[Gledhill, T. M.; Hindson, L.; Thompson, M. A.] Univ Hertfordshire, Sci & Technol Res Inst, Hatfield AL10 9AB, Herts, England.
[Goldsmith, P. F.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Jackson, J. M.] Boston Univ, Dept Astron, Boston, MA 02215 USA.
[Kurtz, S. E.] Univ Nacl Autonoma Mexico, Ctr Radioastron & Astrofis, Morelia 58090, Michoacan, Mexico.
[Marti, J.] Univ Jaen, Dept Fis, EPSJ, E-23071 Jaen, Spain.
[Moore, T. J. T.] Liverpool John Moores Univ, Astrophys Res Inst, Birkenhead CH41 1LD, Merseyside, England.
[Mundy, L. G.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Pandian, J. D.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA.
[Paredes, J. M.] Univ Barcelona UB IEEC, Dept Astron & Meteorol, E-08028 Barcelona, Spain.
[Paredes, J. M.] Univ Barcelona UB IEEC, ICC, E-08028 Barcelona, Spain.
[Shepherd, D. S.] Sq Kilometre Array South Africa, ZA-7405 Cape Town, Western Cape, South Africa.
[Umana, G.] INAF Osservatorio Astrofis Catania, I-95123 Catania, Italy.
RP Purcell, CR (reprint author), Univ Leeds, Sch Phys & Astron, EC Stoner Bldg, Leeds LS2 9JT, W Yorkshire, England.
EM C.R.Purcell@leeds.ac.uk
RI Goldsmith, Paul/H-3159-2016;
OI Muxlow, Thomas/0000-0001-5797-8796; Umana, Grazia/0000-0002-6972-8388;
Purcell, Cormac/0000-0002-7491-7386; Paredes, Josep
M./0000-0002-1566-9044
FU STFC
FX The authors thank the referee, Jim Condon, for his thorough comments
which very much improved the quality of the paper. We also thank the
Director and staff of the VLA for their assistance during the
preparation of these observations. Thanks also to James Alison for many
helpful discussions. C.R.P. was supported by a STFC postdoctoral grant
while at the Universities of Manchester and Leeds.
NR 41
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U1 5
U2 30
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0067-0049
J9 ASTROPHYS J SUPPL S
JI Astrophys. J. Suppl. Ser.
PD MAR
PY 2013
VL 205
IS 1
AR 1
DI 10.1088/0067-0049/205/1/1
PG 22
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 100EC
UT WOS:000315677600001
ER
PT J
AU Sandford, SA
Bernstein, MP
Materese, CK
AF Sandford, Scott A.
Bernstein, Max P.
Materese, Christopher K.
TI THE INFRARED SPECTRA OF POLYCYCLIC AROMATIC HYDROCARBONS WITH EXCESS
PERIPHERAL H ATOMS (H-n-PAHs) AND THEIR RELATION TO THE 3.4 AND 6.9 mu m
PAH EMISSION FEATURES
SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES
LA English
DT Article
DE infrared: ISM; ISM: abundances; ISM: lines and bands; ISM: molecules;
methods: laboratory; molecular data; techniques: spectroscopic
ID INTERPLANETARY DUST PARTICLES; DEUTERIUM ENRICHMENT; PERDEUTERATED
NAPHTHALENE; MURCHISON METEORITE; ABSORPTION-SPECTRA; IRAS SOURCES;
SPECTROSCOPY; CATIONS; ULTRAVIOLET; MOLECULES
AB Polycyclic aromatic hydrocarbons (PAHs) are likely responsible for the family of infrared emission features seen in a wide variety of astrophysical environments. A potentially important subclass of these materials are PAHs whose edges contain excess H atoms (Hn-PAHs). This type of compound may be present in space, but it has been difficult to assess this possibility because of a lack of suitable laboratory spectra to assist with analysis of astronomical data. We present 4000-500 cm(-1) (2.5-20 mu m) infrared spectra of 23 Hn-PAHs and related molecules isolated in argon matrices under conditions suitable for interpretation of astronomical data. Spectra of molecules with mixed aromatic and aliphatic domains show characteristics that distinguish them from fully aromatic PAH equivalents. Two major changes occur as PAHs become more hydrogenated: (1) aromatic C-H stretching bands near 3.3 mu m weaken and are replaced with stronger aliphatic bands near 3.4 mu m, and (2) aromatic C-H out-of-plane bending mode bands in the 11-15 mu m region shift and weaken concurrent with growth of a strong aliphatic -CH2-deformation mode near 6.9 mu m. Implications for interpreting astronomical spectra are discussed with emphasis on the 3.4 and 6.9 mu m features. Laboratory data is compared with emission spectra from IRAS 21282+5050, an object with normal PAH emission features, and IRAS 22272+5435 and IRAS 0496+3429, two protoplanetary nebulae with abnormally large 3.4 mu m features. We show that "normal" PAH emission objects contain relatively few Hn-PAHs in their emitter populations, but less evolved protoplanetary nebulae may contain significant abundances of these molecules.
C1 [Sandford, Scott A.; Bernstein, Max P.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Bernstein, Max P.] NASA Headquarters, Washington, DC 20546 USA.
[Materese, Christopher K.] SETI Inst, Mountain View, CA 94043 USA.
RP Sandford, SA (reprint author), NASA, Ames Res Ctr, Mail Stop 245-6, Moffett Field, CA 94035 USA.
EM Scott.A.Sandford@nasa.gov
FU NASA
FX The authors would like to thank C. Bauschlicher, L. Allamandola, A.
Mattioda, and an anonymous reviewer for helpful comments and suggestions
provided during the very long duration of this work. We would like to
thank D. Hudgins for providing the previously unpublished spectrum of
benzo[a]pyrene. We are also grateful to J. Dworkin for doing HPLC work
to establish the purity of several of our compounds. The paper also
benefited greatly from excellent technical support by R. Walker. We are
also grateful to M. Vala and J. Szczepanski for kindly providing us with
their spectral data for fluorine (Szczepanski et al. 2002) which appears
in the Appendix. Finally, the authors are grateful for funding from NASA
grants from the Origins of Solar Systems, Exobiology, Astrobiology, and
Astrophysics Programs, which made this work possible.
NR 49
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U1 2
U2 15
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0067-0049
J9 ASTROPHYS J SUPPL S
JI Astrophys. J. Suppl. Ser.
PD MAR
PY 2013
VL 205
IS 1
AR 8
DI 10.1088/0067-0049/205/1/8
PG 30
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 100EC
UT WOS:000315677600008
ER
PT J
AU Reid, JS
Hyer, EJ
Johnson, RS
Holben, BN
Yokelson, RJ
Zhang, JL
Campbell, JR
Christopher, SA
Di Girolamo, L
Giglio, L
Holz, RE
Kearney, C
Miettinen, J
Reid, EA
Turk, FJ
Wang, J
Xian, P
Zhao, GY
Balasubramanian, R
Chew, BN
Janjai, S
Lagrosas, N
Lestari, P
Lin, NH
Mahmud, M
Nguyen, AX
Norris, B
Oanh, NTK
Oo, M
Salinas, SV
Welton, EJ
Liew, SC
AF Reid, Jeffrey S.
Hyer, Edward J.
Johnson, Randall S.
Holben, Brent N.
Yokelson, Robert J.
Zhang, Jianglong
Campbell, James R.
Christopher, Sundar A.
Di Girolamo, Larry
Giglio, Louis
Holz, Robert E.
Kearney, Courtney
Miettinen, Jukka
Reid, Elizabeth A.
Turk, F. Joseph
Wang, Jun
Xian, Peng
Zhao, Guangyu
Balasubramanian, Rajasekhar
Chew, Boon Ning
Janjai, Serm
Lagrosas, Nofel
Lestari, Puji
Lin, Neng-Huei
Mahmud, Mastura
Nguyen, Anh X.
Norris, Bethany
Oanh, Nguyen T. K.
Oo, Min
Salinas, Santo V.
Welton, E. Judd
Liew, Soo Chin
TI Observing and understanding the Southeast Asian aerosol system by remote
sensing: An initial review and analysis for the Seven Southeast Asian
Studies (7SEAS) program
SO ATMOSPHERIC RESEARCH
LA English
DT Review
DE Southeast Asia; Maritime Continent; Meteorology; Aerosol
ID BIOMASS-BURNING EMISSIONS; INDONESIAN FOREST-FIRES; OPTICAL TRANSIENT
DETECTOR; PHOTOSYNTHETICALLY ACTIVE RADIATION; BANGKOK METROPOLITAN
REGION; OZONE MAPPING SPECTROMETER; MADDEN-JULIAN OSCILLATION;
INDIVIDUAL AVHRR CHANNELS; CHEMICAL-TRANSPORT MODEL; PEAT SWAMP FOREST
AB Southeast Asia (SEA) hosts one of the most complex aerosol systems in the world, with convoluted meteorological scales, sharp geographic and socioeconomic features, high biological productivity, mixtures of a wide range of atmospheric pollutants, and likely a significant susceptibility to global climate change. This physical complexity of SEA is coupled with one of the world's most challenging environments for both in situ and remote sensing observation. The 7-Southeast Asian Studies (7SEAS) program was formed to facilitate interdisciplinary research into the integrated SEA aerosol environment via grass roots style collaboration. In support of the early 7SEAS program and the affiliated Southeast Asia Composition, Cloud, Climate Coupling Regional Study (SEAC(4)RS), this review was created to outline the network of connections linking aerosol particles in SEA with meteorology, climate and the total earth system. In this review, we focus on and repeatedly link back to our primary data source: satellite aerosol remote sensing and associated observability issues. We begin with a brief rationale for the program, outlining key aerosol impacts and, comparing their magnitudes to the relative uncertainty of observations. We then discuss aspects of SEA's physical, socio-economic and biological geography relevant to meteorology and observability issues associated with clouds and precipitation. We show that not only does SEA pose significant observability challenges for aerosol particles, but for clouds and precipitation as well. With the fundamentals of the environment outlined, we explore SEA's most studied aerosol issue: biomass burning. We summarize research on bulk aerosol properties for SEA, including a short synopsis of recent AERONET observations. We describe long range transport patterns. Finally, considerable attention is paid to satellite aerosol observability issues, with a face value comparison of common aerosol products in the region including passive and active aerosol products as well as fluxes. We show that satellite data products diverge greatly due to a host of known artifacts. These artifacts have important implications for how research is conducted, and care must be taken when using satellite products to study aerosol problems. The paper ends with a discussion of how the community can approach this complex and important environment. Published by Elsevier B.V.
C1 [Reid, Jeffrey S.; Hyer, Edward J.; Campbell, James R.; Reid, Elizabeth A.] USN, Marine Meteorol Div, Res Lab, Monterey, CA 93943 USA.
[Johnson, Randall S.; Zhang, Jianglong] Univ N Dakota, Dept Atmospher Sci, Grand Forks, ND 58201 USA.
[Holben, Brent N.; Welton, E. Judd] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Yokelson, Robert J.] Univ Montana, Dept Chem, Missoula, MT 59812 USA.
[Christopher, Sundar A.] Univ Alabama, Dept Atmospher Sci, Huntsville, AL 35899 USA.
[Di Girolamo, Larry; Zhao, Guangyu; Norris, Bethany] Univ Illinois, Dept Atmospher Sci, Urbana, IL 61801 USA.
[Giglio, Louis] Univ Maryland, Dept Geog, College Pk, MD 20742 USA.
[Holz, Robert E.; Oo, Min] Univ Wisconsin, Ctr Space Sci & Engn, Madison, WI 53706 USA.
[Kearney, Courtney] USN, Ocean Sci Div, Res Lab, Stennis, MS USA.
[Miettinen, Jukka; Chew, Boon Ning; Salinas, Santo V.; Liew, Soo Chin] Natl Univ Singapore, Ctr Remote Imaging Sensing & Proc, Singapore 117548, Singapore.
[Turk, F. Joseph] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Wang, Jun] Univ Nebraska, Dept Atmospher Sci, Lincoln, NE USA.
[Xian, Peng] USN, Res Lab, Monterey, CA USA.
[Balasubramanian, Rajasekhar] Natl Univ Singapore, Dept Civil & Environm Engn, Singapore 117548, Singapore.
[Janjai, Serm] Silpakorn Univ, Dept Phys, Nakhon Pathom, Thailand.
[Lagrosas, Nofel] Ateneo Manila Univ, Manila Observ, Quezon City, Philippines.
[Lestari, Puji] Bandung Inst Technol, Dept Environm Engn, Bandung, Indonesia.
[Lin, Neng-Huei] Natl Cent Univ, Dept Atmospher Sci, Chungli 32054, Taiwan.
[Mahmud, Mastura] Univ Kebangsaan Malaysia, Earth Observat Ctr, Babangi Selangor, Malaysia.
[Nguyen, Anh X.] Acad Sci & Technol, Inst Geophys, Hanoi, Vietnam.
[Oanh, Nguyen T. K.] Asian Inst Technol, Dept Environm Engn & Management, Klongluang, Thailand.
RP Reid, JS (reprint author), USN, Marine Meteorol Div, Res Lab, 7 Grace Hopper Ave,Stop 2, Monterey, CA 93943 USA.
EM jeffrey.reid@nrlmry.navy.mil
RI Campbell, James/C-4884-2012; Liew, Soo Chin/C-9187-2011; Eclevia,
Marian/I-6486-2013; Balasubramanian, Rajasekhar/C-2243-2011; Reid,
Jeffrey/B-7633-2014; Yokelson, Robert/C-9971-2011; Hyer,
Edward/E-7734-2011; Wang, Jun/A-2977-2008; Chew, Boon Ning/M-2405-2016
OI LAGROSAS, NOFEL/0000-0002-8672-4717; Campbell,
James/0000-0003-0251-4550; Liew, Soo Chin/0000-0001-8342-4682;
Balasubramanian, Rajasekhar/0000-0002-5627-3628; Reid,
Jeffrey/0000-0002-5147-7955; Yokelson, Robert/0000-0002-8415-6808; Hyer,
Edward/0000-0001-8636-2026; Wang, Jun/0000-0002-7334-0490; Chew, Boon
Ning/0000-0002-2933-7788
FU Naval Research Laboratory Base Program; NASA Interdisciplinary Science
Program; Office of Naval Research [32]; National Aeronautics and Space
Administration; Jet Propulsion Laboratory; program for
application-oriented fundamental research projects (Ministry of Science
and Technology)
FX This paper was compiled with the efforts of many individuals on the 7
Southeast Asian Studies team across Southeast Asia and the United
States. Funding for the construction of this review was predominantly
through the Naval Research Laboratory Base Program and the NASA
Interdisciplinary Science Program. We are grateful to the AERONET
program and its members for the use of Southeast Asian regional data.
Randall Johnson and Jianglong Zhang were supported by the Office of
Naval Research Code 32. James Campbell was supported by the Office of
Naval Research Code 32. F. Joseph Turk's contribution was performed at
the Jet Propulsion Laboratory, under a contract with the National
Aeronautics and Space Administration. Larry Di Girolamo was partially
supported under contract with the Jet Propulsion Laboratory. Vietnam
funding provided by the program for application-oriented fundamental
research projects (Ministry of Science and Technology). We would like to
thank Ralph Kahn and Andrew Sayer (NASA GSFC) for helpful comments. We
are very grateful to the two anonymous reviewers for taking the time to
perform a thorough review of this long manuscript and making many
helpful suggestions. Finally, we remember our friend and colleague, Dr.
Greg Leptoukh who recently passed away. He was instrumental in creating
innovative ways to visualize and analyze satellite aerosol products. He
will be greatly missed.
NR 498
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U2 123
PU ELSEVIER SCIENCE INC
PI NEW YORK
PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA
SN 0169-8095
EI 1873-2895
J9 ATMOS RES
JI Atmos. Res.
PD MAR
PY 2013
VL 122
BP 403
EP 468
DI 10.1016/j.atmosres.2012.06.005
PG 66
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 098LT
UT WOS:000315551500032
ER
PT J
AU Campbell, JR
Reid, JS
Westphal, DL
Zhang, JL
Tackett, JL
Chew, BN
Welton, EJ
Shimizu, A
Sugimoto, N
Aoki, K
Winker, DM
AF Campbell, James R.
Reid, Jeffrey S.
Westphal, Douglas L.
Zhang, Jianglong
Tackett, Jason L.
Chew, Boon Ning
Welton, Ellsworth J.
Shimizu, Atsushi
Sugimoto, Nobuo
Aoki, Kazuma
Winker, David M.
TI Characterizing the vertical profile of aerosol particle extinction and
linear depolarization over Southeast Asia and the Maritime Continent:
The 2007-2009 view from CALIOP
SO ATMOSPHERIC RESEARCH
LA English
DT Article
DE CALIPSO; Lidar; Southeast Asia; Maritime Continent; Aerosol particle
scattering; Aerosol composition
ID OPTICAL DEPTH; DATA-ASSIMILATION; TROPOSPHERIC AEROSOLS; LIDAR
OBSERVATIONS; RADIATIVE IMPACTS; SUMMER MONSOON; MODIS; CALIPSO; CLOUD;
SATELLITE
AB Vertical profiles of 0.532 mu m aerosol particle extinction coefficient and linear volume depolarization ratio are described for Southeast Asia and the Maritime Continent Quality-screened and cloud-cleared Version 3.01 Level 2 NASA Cloud Aerosol Lidar with Orthogonal Polarization (CALIOP) 5-km Aerosol Profile datasets are analyzed from 2007 to 2009. Numerical simulations from the U.S. Naval Aerosol Analysis and Predictive System (NAAPS), featuring two-dimensional variational assimilation of NASA Moderate Resolution Imaging Spectroradiometer and Multi-angle Imaging Spectra-Radiometer quality-assured datasets, combined with regional ground-based lidar measurements, are considered for assessing CALIOP retrieval performance, identifying bias, and evaluating regional representativeness. CALIOP retrievals of aerosol particle extinction coefficient and aerosol optical depth (AOD) are high over land and low over open waters relative to NAAPS (0.412/0.312 over land for all data points inclusive, 0.310/0.235 when the per bin average is used and each is treated as single data points; 0.102/0.151 and 0.086/0.124, respectively, over ocean). Regional means, however, are very similar (0.180/0.193 for all data points and 0.155/0.159 when averaged per normalized bin), as the two factors offset one another. The land/ocean offset is investigated, and discrepancies attributed to interpretation of particle composition and a-priori assignment of the extinction-to-backscatter ratio ("lidar ratio") necessary for retrieving the extinction coefficient from CALIOP signals. Over land, NAAPS indicates more dust present than CALIOP algorithms are identifying, indicating a likely assignment of a higher lidar ratio representative of more absorptive particles. NAAPS resolves more smoke over water than identified with CALIOP, indicating likely usage of a lidar ratio characteristic of less absorptive particles to be applied that biases low AOD there. Over open waters except within the Bay of Bengal, aerosol particle scattering is largely capped below 1.5 km MSL, though ground-based lidar measurements at Singapore differ slightly from this finding. Significant aerosol particle presence over land is similarly capped near 3.0 km MSL over most regions. Particle presence at low levels regionally, except over India, is dominated by relatively non-depolarizing particles. Industrial haze, sea salt droplets and fresh smoke are thus most likely present Published by Elsevier B.V.
C1 [Campbell, James R.; Reid, Jeffrey S.; Westphal, Douglas L.] USN, Aerosol & Radiat Sci Sect, Marine Meteorol Div, Res Lab, Monterey, CA 93943 USA.
[Zhang, Jianglong] Univ N Dakota, Dept Atmospher Sci, Grand Folks, ND USA.
[Tackett, Jason L.] NASA, Langley Res Ctr, Sci Syst & Applicat Inc, Hampton, VA 23665 USA.
[Chew, Boon Ning] Natl Univ Singapore, Ctr Remote Imaging Sensing & Proc, Singapore 117548, Singapore.
[Welton, Ellsworth J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Shimizu, Atsushi; Sugimoto, Nobuo] Natl Inst Environm Studies, Tsukuba, Ibaraki, Japan.
[Aoki, Kazuma] Toyama Univ, Dept Earth Sci, Toyama 930, Japan.
[Winker, David M.] NASA, Langley Res Ctr, Hampton, VA 23665 USA.
RP Campbell, JR (reprint author), USN, Aerosol & Radiat Sci Sect, Marine Meteorol Div, Res Lab, Monterey, CA 93943 USA.
EM james.campbell@nrlmry.navy.mil
RI Campbell, James/C-4884-2012; Reid, Jeffrey/B-7633-2014; Shimizu,
Atsushi/C-2810-2009; Sugimoto, Nobuo/C-5189-2015; Chew, Boon
Ning/M-2405-2016
OI Campbell, James/0000-0003-0251-4550; Reid, Jeffrey/0000-0002-5147-7955;
Shimizu, Atsushi/0000-0002-7306-7412; Sugimoto,
Nobuo/0000-0002-0545-1316; Chew, Boon Ning/0000-0002-2933-7788
FU Office of Naval Research [35]; NASA Interagency Agreement on behalf of
the Micropulse Lidar Network (MPLNET) [NNG11HG12I]
FX This research was funded by the Office of Naval Research Code 35. Author
JRC acknowledges the support of NASA Interagency Agreement NNG11HG12I on
behalf of the Micropulse Lidar Network (MPLNET). MPLNET is operated with
the support of the NASA Radiation Sciences Program. The authors thank
Mark A. Vaughan at NASA Langley Research Center with his help
interpreting the CALIOP Level 2.0 Aerosol Profile datasets. The group
acknowledges the NASA AERONET program, their contributing principal
investigators and staff for coordinating the coastal and inland sites
used in this investigation.
NR 94
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U1 4
U2 42
PU ELSEVIER SCIENCE INC
PI NEW YORK
PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA
SN 0169-8095
EI 1873-2895
J9 ATMOS RES
JI Atmos. Res.
PD MAR
PY 2013
VL 122
BP 520
EP 543
DI 10.1016/j.atmosres.2012.05.007
PG 24
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 098LT
UT WOS:000315551500036
ER
PT J
AU Salinas, SV
Chew, BN
Miettinen, J
Campbell, JR
Welton, EJ
Reid, JS
Yu, LYE
Liew, SC
AF Salinas, Santo V.
Chew, Boon Ning
Miettinen, Jukka
Campbell, James R.
Welton, Ellsworth J.
Reid, Jeffrey S.
Yu, Liya E.
Liew, Soo Chin
TI Physical and optical characteristics of the October 2010 haze event over
Singapore: A photometric and lidar analysis
SO ATMOSPHERIC RESEARCH
LA English
DT Article
DE Aerosols; Haze; Air quality; AERONET; MPLNET; South East Asia
ID BIOMASS BURNING AEROSOLS; DIRECT SUN DATA; EL-NINO; FOREST-FIRES;
AIR-QUALITY; INDONESIA; DEPTH; SMOKE; AERONET; IMPACT
AB Trans-boundary biomass burning smoke episodes have increased dramatically during the past 20-30 years and have become an annual phenomenon in the South-East-Asia region. On 15th October 2010, elevated levels of fire activity were detected by remote sensing satellites (e.g. MODIS). On the same date, measurements of fine particulate matter (PM2.5) at Singapore and Malaysia found high levels of fine mode particles in the local environment. All these observations were indicative of the initial onset of a smoke episode that lasted for several days. In this work, we investigate the temporal evolution of this smoke episode by analyzing the physical and optical properties of smoke particles with the aid of an AERONET Sun photometer, an MPLNet micropulse lidar, and surface PM2.5 measurements. Elevated levels of fire activity coupled with high aerosol optical depth and PM2.5 were observed over a period of nine days. Increased variability of parameters such as aerosol optical depth, Angstrom exponent number and its fine mode equivalents all indicated high levels of fine particulate presence in the atmosphere. Smoke particle growth due to aging, coagulation and condensation mechanisms was detected during the afternoons and over several days. Retrieved lidar ratios were compatible with the presence of fine particulate within the boundary/aerosol layer. Moreover, retrieved particle size distribution as well as single scattering albedo indicated the prevalence of the fine mode particulate regime as well as particles showing enhanced levels of absorption respectively. (C) 2012 Elsevier B.V. All rights reserved.
C1 [Salinas, Santo V.; Chew, Boon Ning; Miettinen, Jukka; Liew, Soo Chin] Natl Univ Singapore, CRISP, Singapore 119076, Singapore.
[Campbell, James R.] NASA, Goddard Space Flight Ctr, Sigma Space Corp, Greenbelt, MD 20771 USA.
[Welton, Ellsworth J.] NASA, Goddard Space Flight Ctr, Micropulse Lidar Network, Greenbelt, MD 20771 USA.
[Reid, Jeffrey S.] USN, Res Lab, Marine Meteorol Div, Monterey, CA 93943 USA.
[Yu, Liya E.] Natl Univ Singapore, Dept Civil & Environm Engn, Singapore 119076, Singapore.
RP Salinas, SV (reprint author), Natl Univ Singapore, CRISP, Block S17,Level 2,10 Lower Kent Ridge Rd, Singapore 119076, Singapore.
EM crsscsv@nus.edu.sg
RI Campbell, James/C-4884-2012; Yu, Liya/H-2573-2013; Liew, Soo
Chin/C-9187-2011; Reid, Jeffrey/B-7633-2014; Xiongfei, Zhao/G-7690-2015;
Chew, Boon Ning/M-2405-2016
OI Campbell, James/0000-0003-0251-4550; Yu, Liya/0000-0001-9182-6593; Liew,
Soo Chin/0000-0001-8342-4682; Reid, Jeffrey/0000-0002-5147-7955; Chew,
Boon Ning/0000-0002-2933-7788
FU Agency for Science, Technology & Research (A*STAR) of Singapore
FX The authors would like to thank AERONET and MPLNET for processing and
archiving the Sun photometer and lidar data. CRISP would like to thank
the Agency for Science, Technology & Research (A*STAR) of Singapore for
Financial support.
NR 60
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PU ELSEVIER SCIENCE INC
PI NEW YORK
PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA
SN 0169-8095
EI 1873-2895
J9 ATMOS RES
JI Atmos. Res.
PD MAR
PY 2013
VL 122
BP 555
EP 570
DI 10.1016/j.atmosres.2012.05.021
PG 16
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 098LT
UT WOS:000315551500038
ER
PT J
AU Turk, FJ
Xian, P
AF Turk, F. Joseph
Xian, Peng
TI An assessment of satellite-based high resolution precipitation datasets
for atmospheric composition studies in the maritime continent
SO ATMOSPHERIC RESEARCH
LA English
DT Article
DE Precipitation; Aerosol; TRMM; GPM; MODIS
ID PASSIVE MICROWAVE; RAINFALL; SMOKE; TRANSPORT; AEROSOLS; REGIONS; ASIA
AB The Maritime Continent (MC) region of Southeast Asia is known for land use practices that are modulated by precipitation occurrence and fire activity. The polluted environment may modify cloud/precipitation formation mechanisms, but meteorological or weather patterns may disrupt or otherwise influence these same processes. Since the simultaneous retrieval of precipitation and aerosol properties is not possible from current satellite observations, the choice of the precipitation dataset used for applications such as model assimilation and scavenging in aerosol transport models could provide very different results. In this article, a seven-year (2003-2009) time period was analyzed with five satellite-based high-resolution precipitation products (HRPP), the MERRA model reanalysis, and MODIS-derived aerosol observations within nine Southeast Asia domains. Substantially different trends between the aerosol concentration and precipitation time series were noted for different MC island regions, as well as HRPP differences in the precipitation diurnal variability and their capability to track precipitation extremes. For all regions, the most noticeable change to the diurnal cycle was noted during the genesis phase (Phase 1 in the MC) of the intraseasonal Madden Julian Oscillation (MJO). Since these studies do not take any aerosol transport or precipitation dynamics into account, the use of Lagrangian models is proposed to study non-localized aerosol/precipitation interactions and better establish their veracity in current model simulations. (C) 2012 Elsevier B.V. All rights reserved.
C1 [Turk, F. Joseph] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Xian, Peng] USN, Res Lab, Marine Meteorol Div, Monterey, CA 93940 USA.
RP Turk, FJ (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM jturk@jpl.nasa.gov
FU NASA; Naval Research Laboratory Base Program; JST-CREST
FX The authors acknowledge support from NASA's Interdisciplinary Science
(IDS) program through Dr. Hal Maring. The first author's work was
performed at the Jet Propulsion Laboratory, California Institute of
Technology, under contract with the National Aeronautics and Space
Administration. The second author acknowledges partial support from the
Naval Research Laboratory Base Program. The GSMaP Project was sponsored
by JST-CREST and is promoted by the JAXA Precipitation Measuring Mission
(PMM) Science Team, and the GSMaP products were distributed by the Earth
Observation Research Center, Japan Aerospace Exploration Agency. The
authors are grateful for the comments provided by the two independent
reviewers.
NR 38
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PU ELSEVIER SCIENCE INC
PI NEW YORK
PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA
SN 0169-8095
J9 ATMOS RES
JI Atmos. Res.
PD MAR
PY 2013
VL 122
BP 579
EP 598
DI 10.1016/j.atmosres.2012.02.017
PG 20
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 098LT
UT WOS:000315551500040
ER
PT J
AU Maruskin, JM
Bellerose, J
Wong, M
Mitchell, L
Richardson, D
Mathews, D
Nguyen, T
Ganeshalingam, U
Ma, G
AF Maruskin, Jared M.
Bellerose, Julie
Wong, Macken
Mitchell, Lara
Richardson, David
Mathews, Douglas
Tri Nguyen
Ganeshalingam, Usha
Ma, Gina
TI Dust motions in quasi-statically charged binary asteroid systems
SO CELESTIAL MECHANICS & DYNAMICAL ASTRONOMY
LA English
DT Article
DE Four body problem; Binary asteroids; Dust motion; Levitation conditions;
Dust levitation; Lofting; Charged debris; Electrostatic force
ID FULL 2-BODY PROBLEM; 1999 KW4; STABILITY; MOON
AB In this paper, we discuss dust motion and investigate possible mass transfer of charged particles in a binary asteroid system, in which the asteroids are electrically charged due to solar radiation. The surface potential of the asteroids is assumed to be a piecewise function, with positive potential on the sunlit half and negative potential on the shadow half. We derive the nonautonomous equations of motion for charged particles and an analytic representation for their lofting conditions. Particle trajectories and temporary relative equilibria are examined in relation to their moving forbidden regions, a concept we define and discuss. Finally, we use a Monte Carlo simulation for a case study on mass transfer and loss rates between the asteroids.
C1 [Maruskin, Jared M.] San Jose State Univ, Dept Math, San Jose, CA 95192 USA.
[Bellerose, Julie] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Wong, Macken; Mitchell, Lara; Richardson, David; Mathews, Douglas; Tri Nguyen; Ganeshalingam, Usha; Ma, Gina] San Jose State Univ, San Jose, CA 95192 USA.
RP Maruskin, JM (reprint author), San Jose State Univ, Dept Math, San Jose, CA 95192 USA.
EM maruskin@math.sjsu.edu
NR 39
TC 1
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U1 0
U2 4
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0923-2958
J9 CELEST MECH DYN ASTR
JI Celest. Mech. Dyn. Astron.
PD MAR
PY 2013
VL 115
IS 3
BP 281
EP 298
DI 10.1007/s10569-012-9465-4
PG 18
WC Astronomy & Astrophysics; Mathematics, Interdisciplinary Applications
SC Astronomy & Astrophysics; Mathematics
GA 104RA
UT WOS:000316011100004
ER
PT J
AU Anderson, RL
Parker, JS
AF Anderson, Rodney L.
Parker, Jeffrey S.
TI Comparison of low-energy lunar transfer trajectories to invariant
manifolds
SO CELESTIAL MECHANICS & DYNAMICAL ASTRONOMY
LA English
DT Article
DE Lunar transfers; Invariant manifolds; Dynamical systems theory;
Libration point orbits; Earth-Moon landing geometry; Lyapunov orbits
ID LIBRATION POINT ORBITS; 3-BODY PROBLEM; FAMILIES; EARTH; MOON
AB In this study, transfer trajectories from the Earth to the Moon that encounter the Moon at various flight path angles are examined, and lunar approach trajectories are compared to the invariant manifolds of selected unstable orbits in the circular restricted three-body problem. Previous work focused on lunar impact and landing trajectories encountering the Moon normal to the surface, and this research extends the problem with different flight path angles in three dimensions. The lunar landing geometry for a range of Jacobi constants is computed, and approaches to the Moon via invariant manifolds from unstable orbits are analyzed for different energy levels.
C1 [Anderson, Rodney L.; Parker, Jeffrey S.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Anderson, RL (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr,M-S 301-121, Pasadena, CA 91109 USA.
EM Rodney.L.Anderson@jpl.nasa.gov; Jeffrey.S.Parker@jpl.nasa.gov
OI Anderson, Rodney/0000-0001-5336-2775
NR 34
TC 7
Z9 7
U1 0
U2 11
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0923-2958
J9 CELEST MECH DYN ASTR
JI Celest. Mech. Dyn. Astron.
PD MAR
PY 2013
VL 115
IS 3
BP 311
EP 331
DI 10.1007/s10569-012-9466-3
PG 21
WC Astronomy & Astrophysics; Mathematics, Interdisciplinary Applications
SC Astronomy & Astrophysics; Mathematics
GA 104RA
UT WOS:000316011100006
ER
PT J
AU Chander, G
Hewison, TJ
Fox, N
Wu, XQ
Xiong, XX
Blackwell, WJ
AF Chander, Gyanesh
Hewison, Tim J.
Fox, Nigel
Wu, Xiangqian
Xiong, Xiaoxiong
Blackwell, William J.
TI Foreword to the Special Issue on Intercalibration of Satellite
Instruments
SO IEEE TRANSACTIONS ON GEOSCIENCE AND REMOTE SENSING
LA English
DT Editorial Material
C1 [Chander, Gyanesh] SGT USGS EROS Ctr, Sioux Falls, SD 57198 USA.
[Hewison, Tim J.] European Org Exploitat Meteorol Satellites EUMETS, Darmstadt, Germany.
[Fox, Nigel] Natl Phys Lab, Teddington TW11 0LW, Middx, England.
[Wu, Xiangqian] STAR NESDIS NOAA, College Pk, MD 20740 USA.
[Xiong, Xiaoxiong] NASA Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Blackwell, William J.] MIT Lincoln Lab, Lexington, MA 02420 USA.
RP Chander, G (reprint author), SGT USGS EROS Ctr, Sioux Falls, SD 57198 USA.
RI Wu, Xiangqian/F-5634-2010;
OI Wu, Xiangqian/0000-0002-7804-5650; Hewison, Tim/0000-0002-7845-5107
NR 0
TC 1
Z9 1
U1 3
U2 18
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 0196-2892
J9 IEEE T GEOSCI REMOTE
JI IEEE Trans. Geosci. Remote Sensing
PD MAR
PY 2013
VL 51
IS 3
SI SI
BP 1052
EP 1055
DI 10.1109/TGRS.2013.2240331
PN 1
PG 4
WC Geochemistry & Geophysics; Engineering, Electrical & Electronic; Remote
Sensing; Imaging Science & Photographic Technology
SC Geochemistry & Geophysics; Engineering; Remote Sensing; Imaging Science
& Photographic Technology
GA 100TI
UT WOS:000315725900001
ER
PT J
AU Chander, G
Hewison, TJ
Fox, N
Wu, XQ
Xiong, XX
Blackwell, WJ
AF Chander, Gyanesh
Hewison, Tim J.
Fox, Nigel
Wu, Xiangqian
Xiong, Xiaoxiong
Blackwell, William J.
TI Overview of Intercalibration of Satellite Instruments
SO IEEE TRANSACTIONS ON GEOSCIENCE AND REMOTE SENSING
LA English
DT Article
DE Calibration; comparison; constellations; correction; cross-calibration;
Earth Observing (EO) System; infrared; intercalibration; international
collaboration; microwave; monitoring; radiometric calibration;
reflective solar band (RSB); satellite; satellites; thermal infrared;
traceability; validation; visible
ID IN-FLIGHT CALIBRATION; ABSOLUTE RADIOMETRIC CALIBRATION; HIGH-RESOLUTION
RADIOMETER; NEAR-INFRARED CHANNELS; ON-ORBIT CALIBRATION; SIMULTANEOUS
NADIR OBSERVATIONS; BRIGHTNESS TEMPERATURE BIASES; ANGULAR-DISTRIBUTION
MODELS; BULK SCATTERING PROPERTIES; RADIATIVE FLUX ESTIMATION
AB Intercalibration of satellite instruments is critical for detection and quantification of changes in the Earth's environment, weather forecasting, understanding climate processes, and monitoring climate and land cover change. These applications use data from many satellites; for the data to be interoperable, the instruments must be cross-calibrated. To meet the stringent needs of such applications, instruments must provide reliable, accurate, and consistent measurements over time. Robust techniques are required to ensure that observations from different instruments can be normalized to a common scale that the community agrees on. The long-term reliability of this process needs to be sustained in accordance with established reference standards and best practices. Furthermore, establishing physical meaning to the information through robust Systeme International d'unites traceable calibration and validation (Cal/Val) is essential to fully understand the parameters under observation. The processes of calibration, correction, stability monitoring, and quality assurance need to be underpinned and evidenced by comparison with "peer instruments" and, ideally, highly calibrated in-orbit reference instruments. Intercalibration between instruments is a central pillar of the Cal/Val strategies of many national and international satellite remote sensing organizations. Intercalibration techniques as outlined in this paper not only provide a practical means of identifying and correcting relative biases in radiometric calibration between instruments but also enable potential data gaps between measurement records in a critical time series to be bridged. Use of a robust set of internationally agreed upon and coordinated inter-calibration techniques will lead to significant improvement in the consistency between satellite instruments and facilitate accurate monitoring of the Earth's climate at uncertainty levels needed to detect and attribute the mechanisms of change. This paper summarizes the state-of-the-art of postlaunch radiometric calibration of remote sensing satellite instruments through intercalibration.
C1 [Chander, Gyanesh] US Geol Survey, SGT Inc, Earth Resources Observat & Sci Ctr, Sioux Falls, SD 57198 USA.
[Hewison, Tim J.] European Org Exploitat Meteorol Satellites, D-64295 Darmstadt, Germany.
[Fox, Nigel] Natl Phys Lab, Teddington TW11 0LW, Middx, England.
[Wu, Xiangqian] NOAA, Natl Environm Satellite Data & Informat Serv, Camp Springs, MD 20746 USA.
[Xiong, Xiaoxiong] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Blackwell, William J.] MIT, Lexington, MA 02420 USA.
RP Chander, G (reprint author), US Geol Survey, SGT Inc, Earth Resources Observat & Sci Ctr, Sioux Falls, SD 57198 USA.
EM gchander@usgs.gov
RI Wu, Xiangqian/F-5634-2010; Richards, Amber/K-8203-2015;
OI Wu, Xiangqian/0000-0002-7804-5650; Hewison, Tim/0000-0002-7845-5107
FU U.S. Geological Survey [G10PC00044]
FX This work was supported by the U.S. Geological Survey under Contract
G10PC00044. Any use of trade, product, or firm names is for descriptive
purposes only and does not imply endorsement by the U. S. Government or
the National Metrology Institutes.
NR 241
TC 50
Z9 52
U1 7
U2 55
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 0196-2892
EI 1558-0644
J9 IEEE T GEOSCI REMOTE
JI IEEE Trans. Geosci. Remote Sensing
PD MAR
PY 2013
VL 51
IS 3
SI SI
BP 1056
EP 1080
DI 10.1109/TGRS.2012.2228654
PN 1
PG 25
WC Geochemistry & Geophysics; Engineering, Electrical & Electronic; Remote
Sensing; Imaging Science & Photographic Technology
SC Geochemistry & Geophysics; Engineering; Remote Sensing; Imaging Science
& Photographic Technology
GA 100TI
UT WOS:000315725900002
ER
PT J
AU Kessler, PD
Killough, BD
Gowda, S
Williams, BR
Chander, G
Qu, M
AF Kessler, Paul D.
Killough, Brian D.
Gowda, Sanjay
Williams, Brian R.
Chander, Gyanesh
Qu, Min
TI CEOS Visualization Environment (COVE) Tool for Intercalibration of
Satellite Instruments
SO IEEE TRANSACTIONS ON GEOSCIENCE AND REMOTE SENSING
LA English
DT Article
DE Acquisition; calibration; CEOS Visualization Environment (COVE);
Committee on Earth Observation Satellites (CEOS); coincident ground
observation; Google; iPad; iPhone; satellites; Simplified General
Perturbation 4 (SGP4); Systems Tool Kit (STK); swath; Working Group on
Calibration and Validation (WGCV)
AB Increasingly, data from multiple instruments are used to gain a more complete understanding of land surface processes at a variety of scales. Intercalibration, comparison, and coordination of satellite instrument coverage areas is a critical effort of international and domestic space agencies and organizations. The Committee on Earth Observation Satellites Visualization Environment (COVE) is a suite of browser-based applications that leverage Google Earth to display past, present, and future satellite instrument coverage areas and coincident calibration opportunities. This forecasting and ground coverage analysis and visualization capability greatly benefits the remote sensing calibration community in preparation for multisatellite ground calibration campaigns or individual satellite calibration studies. COVE has been developed for use by a broad international community to improve the efficiency and efficacy of such calibration planning efforts, whether those efforts require past, present, or future predictions. This paper provides a brief overview of the COVE tool, its validation, accuracies, and limitations with emphasis on the applicability of this visualization tool for supporting ground field campaigns and intercalibration of satellite instruments.
C1 [Kessler, Paul D.; Gowda, Sanjay; Williams, Brian R.; Qu, Min] Analyt Mech Associates Inc, Hampton, VA 23666 USA.
[Killough, Brian D.] NASA, Comm Earth Observat Satellites Syst Engn Off, Langley Res Ctr, Hampton, VA 23681 USA.
[Chander, Gyanesh] US Geol Survey, Stinger Ghaffarian Technol Inc, Earth Resources Observat & Sci Ctr, Sioux Falls, SD 57198 USA.
RP Kessler, PD (reprint author), Analyt Mech Associates Inc, Hampton, VA 23666 USA.
EM P.Kessler@ama-inc.com; Brian.D.Killough@nasa.gov; Gowda@ama-inc.com;
B.Williams@ama-inc.com; gchander@usgs.gov; MinQu@ama-inc.com
FU U.S. Geological Survey [G10PC00044]
FX This work was performed under U.S. Geological Survey contract
G10PC00044.
NR 8
TC 2
Z9 2
U1 1
U2 13
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 0196-2892
J9 IEEE T GEOSCI REMOTE
JI IEEE Trans. Geosci. Remote Sensing
PD MAR
PY 2013
VL 51
IS 3
SI SI
BP 1081
EP 1087
DI 10.1109/TGRS.2012.2235841
PN 1
PG 7
WC Geochemistry & Geophysics; Engineering, Electrical & Electronic; Remote
Sensing; Imaging Science & Photographic Technology
SC Geochemistry & Geophysics; Engineering; Remote Sensing; Imaging Science
& Photographic Technology
GA 100TI
UT WOS:000315725900003
ER
PT J
AU Thome, K
McCorkel, J
Czapla-Myers, J
AF Thome, Kurt
McCorkel, Joel
Czapla-Myers, Jeff
TI In-Situ Transfer Standard and Coincident-View Intercomparisons for
Sensor Cross-Calibration
SO IEEE TRANSACTIONS ON GEOSCIENCE AND REMOTE SENSING
LA English
DT Article
DE Advanced Land Imager (ALI); Advanced Spaceborne Thermal Emission and
Reflection Radiometer (ASTER); cross-calibration; Enhanced Thematic
Mapper Plus (ETM plus ); Moderate Resolution Imaging Spectroradiometer
(MODIS); SI-traceability; Thematic Mapper (TM); vicarious calibration
ID IMAGING SPECTRORADIOMETER MODIS; VICARIOUS CALIBRATION; AVHRR; ASTER;
ETM+
AB There exist numerous methods for accomplishing on-orbit calibration. Methods include the reflectance-based approach relying on measurements of surface and atmospheric properties at the time of a sensor overpass as well as invariant scene approaches relying on knowledge of the temporal characteristics of the site. The current work examines typical cross-calibration methods and discusses the expected uncertainties of the methods. Data from the Advanced Land Imager (ALI), Advanced Spaceborne Thermal Emission and Reflection and Radiometer (ASTER), Enhanced Thematic Mapper Plus (ETM+), Moderate Resolution Imaging Spectroradiometer (MODIS), and Thematic Mapper (TM) are used to demonstrate the limits of relative sensor-to-sensor calibration as applied to current sensors while Landsat-5 TM and Landsat-7 ETM+ are used to evaluate the limits of in situ site characterizations for SI-traceable cross calibration. The current work examines the difficulties in trending of results from cross-calibration approaches taking into account sampling issues, site-to-site variability, and accuracy of the method. Special attention is given to the differences caused in the cross-comparison of sensors in radiance space as opposed to reflectance space. The results show that cross calibrations with absolute uncertainties <1.5% (1 sigma) are currently achievable even for sensors without coincident views.
C1 [Thome, Kurt; McCorkel, Joel] NASA, Space & Earth Sci Directorate, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Czapla-Myers, Jeff] Univ Arizona, Coll Opt Sci, Tucson, AZ 85721 USA.
RP Thome, K (reprint author), NASA, Space & Earth Sci Directorate, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
EM kurtis.thome@nasa.gov; joel.mccorkel@nasa.gov;
j.czapla-myers@optics.arizona.edu
RI McCorkel, Joel/D-4454-2012; Thome, Kurtis/D-7251-2012;
OI McCorkel, Joel/0000-0003-2853-2036; Czapla-Myers,
Jeffrey/0000-0003-4804-5358
NR 22
TC 2
Z9 2
U1 4
U2 28
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 0196-2892
J9 IEEE T GEOSCI REMOTE
JI IEEE Trans. Geosci. Remote Sensing
PD MAR
PY 2013
VL 51
IS 3
SI SI
BP 1088
EP 1097
DI 10.1109/TGRS.2013.2243841
PN 1
PG 10
WC Geochemistry & Geophysics; Engineering, Electrical & Electronic; Remote
Sensing; Imaging Science & Photographic Technology
SC Geochemistry & Geophysics; Engineering; Remote Sensing; Imaging Science
& Photographic Technology
GA 100TI
UT WOS:000315725900004
ER
PT J
AU Doelling, DR
Morstad, D
Scarino, BR
Bhatt, R
Gopalan, A
AF Doelling, David R.
Morstad, Daniel
Scarino, Benjamin R.
Bhatt, Rajendra
Gopalan, Arun
TI The Characterization of Deep Convective Clouds as an Invariant
Calibration Target and as a Visible Calibration Technique
SO IEEE TRANSACTIONS ON GEOSCIENCE AND REMOTE SENSING
LA English
DT Article
DE Aqua MODerate Resolution Imaging Spectroradiometer (MODIS); deep
convective clouds (DCCs); pseudoinvariant calibration targets; visible
imager calibration
ID DIURNAL-VARIATIONS; INFRARED CHANNELS; SATELLITE; SCIAMACHY; ATMOSPHERE;
TERRA; MODIS; VIRS; TRMM
AB Deep convective clouds (DCCs) are ideal visible calibration targets because they are bright nearly isotropic solar reflectors located over the tropics and they can be easily identified using a simple infrared threshold. Because all satellites view DCCs, DCCs provide the opportunity to uniformly monitor the stability of all operational sensors, both historical and present. A collective DCC anisotropically corrected radiance calibration approach is used to construct monthly probability distribution functions (PDFs) to monitor sensor stability. The DCC calibration targets were stable to within 0.5% and 0.3% per decade when the selection criteria were optimized based on Aqua MODerate Resolution Imaging Spectroradiometer 0.65-mu m-band radiances. The Tropical Western Pacific (TWP), African, and South American regions were identified as the dominant DCC domains. For the 0.65-mu m band, the PDF mode statistic is preferable, providing 0.3% regional consistency and 1% temporal uncertainty over land regions. It was found that the DCC within the TWP had the lowest radiometric response and DCC over land did not necessarily have the highest radiometric response. For wavelengths greater than 1 mu m, the mean statistic is preferred, and land regions provided a regional variability of 0.7% with a temporal uncertainty of 1.1% where the DCC land response was higher than the response over ocean. Unlike stratus and cirrus clouds, the DCC spectra were not affected by water vapor absorption.
C1 [Doelling, David R.] NASA, Climate Sci Branch, Langley Res Ctr, Hampton, VA 23681 USA.
[Morstad, Daniel; Scarino, Benjamin R.; Bhatt, Rajendra; Gopalan, Arun] Sci Syst & Applicat Inc, Hampton, VA 23666 USA.
RP Doelling, DR (reprint author), NASA, Climate Sci Branch, Langley Res Ctr, Hampton, VA 23681 USA.
EM david.r.doelling@nasa.gov; Daniel.morstad@nasa.gov;
Benjamin.r.scarino@nasa.gov; rajendra.bhatt@nasa.gov;
arun.gopalan-1@nasa.gov
FU NASA CERES program; NASA Satellite Intercalibration Consistency program;
NOAA NCDC SDS Climate Data Records program [IA1-1016]
FX This work was supported by the NASA CERES program, the NASA Satellite
Intercalibration Consistency program, and the NOAA NCDC SDS Climate Data
Records program IA1-1016.
NR 27
TC 30
Z9 30
U1 1
U2 10
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 0196-2892
J9 IEEE T GEOSCI REMOTE
JI IEEE Trans. Geosci. Remote Sensing
PD MAR
PY 2013
VL 51
IS 3
SI SI
BP 1147
EP 1159
DI 10.1109/TGRS.2012.2225066
PN 1
PG 13
WC Geochemistry & Geophysics; Engineering, Electrical & Electronic; Remote
Sensing; Imaging Science & Photographic Technology
SC Geochemistry & Geophysics; Engineering; Remote Sensing; Imaging Science
& Photographic Technology
GA 100TI
UT WOS:000315725900009
ER
PT J
AU Doelling, DR
Scarino, BR
Morstad, D
Gopalan, A
Bhatt, R
Lukashin, C
Minnis, P
AF Doelling, David R.
Scarino, Benjamin R.
Morstad, Daniel
Gopalan, Arun
Bhatt, Rajendra
Lukashin, Constantine
Minnis, Patrick
TI The Intercalibration of Geostationary Visible Imagers Using Operational
Hyperspectral SCIAMACHY Radiances
SO IEEE TRANSACTIONS ON GEOSCIENCE AND REMOTE SENSING
LA English
DT Article
DE Geostationary visible imager calibration; Scanning Imaging Absorption
Spectrometer for Atmospheric Cartography (SCIAMACHY); spectral band
adjustment factor (SBAF)
ID CALIBRATION; RANGE; AIRS; GOME
AB Spectral band differences between sensors can complicate the process of intercalibration of a visible sensor against a reference sensor. This can be best addressed by using a hyperspectral reference sensor whenever possible because they can be used to accurately mitigate the band differences. This paper demonstrates the feasibility of using operational Scanning Imaging Absorption Spectrometer for Atmospheric Cartography (SCIAMACHY) large-footprint hyperspectral radiances to calibrate geostationary Earth-observing (GEO) sensors. Near simultaneous nadir overpass measurements were used to compare the temporal calibration of SCIAMACHY with Aqua Moderate Resolution Imaging Spectroradiometer band radiances, which were found to be consistent to within 0.44% over seven years. An operational SCIAMACHY/GEO ray-matching technique was presented, along with enhancements to improve radiance pair sampling. These enhancements did not bias the underlying intercalibration and provided enough sampling to allow up to monthly monitoring of the GEO sensor degradation. The results of the SCIAMACHY/GEO intercalibration were compared with other operational four-year Meteosat-9 0.65-mu m calibration coefficients and were found to be within 1% of the gain, and more importantly, it had one of the lowest temporal standard errors of all the methods. This is more than likely that the GEO spectral response function could be directly applied to the SCIAMACHY radiances, whereas the other operational methods inferred a spectral correction factor. This method allows the validation of the spectral corrections required by other methods.
C1 [Doelling, David R.; Lukashin, Constantine; Minnis, Patrick] NASA, Climate Sci Branch, Langley Res Ctr, Hampton, VA 23681 USA.
[Scarino, Benjamin R.; Morstad, Daniel; Gopalan, Arun; Bhatt, Rajendra] Sci Syst & Applicat Inc, Hampton, VA 23666 USA.
RP Doelling, DR (reprint author), NASA, Climate Sci Branch, Langley Res Ctr, Hampton, VA 23681 USA.
EM david.r.doelling@nasa.gov; Benjamin.r.scarino@nasa.gov;
Daniel.morstad@nasa.gov; arun.gopalan-1@nasa.gov;
Rajendra.Bhatt@nasa.gov; constantine.lukashin-1@nasa.gov;
p.minnis@nasa.gov
RI Richards, Amber/K-8203-2015; Minnis, Patrick/G-1902-2010
OI Minnis, Patrick/0000-0002-4733-6148
FU National Aeronautics and Space Administration Earth Science Enterprise
Office through the Climate Absolute Radiance and Refractivity
Observatory, Clouds and the Earth's Radiant Energy System; Satellite
Calibration Interconsistency Programs; National Atmospheric and Oceanic
Administration [MOA IA1-1016]
FX This work was supported in part by the National Aeronautics and Space
Administration Earth Science Enterprise Office through the Climate
Absolute Radiance and Refractivity Observatory, Clouds and the Earth's
Radiant Energy System, the Satellite Calibration Interconsistency
Programs and in part by the National Atmospheric and Oceanic
Administration through the Climate Data Records Program under Grant MOA
IA1-1016.
NR 19
TC 8
Z9 8
U1 0
U2 13
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 0196-2892
J9 IEEE T GEOSCI REMOTE
JI IEEE Trans. Geosci. Remote Sensing
PD MAR
PY 2013
VL 51
IS 3
SI SI
BP 1245
EP 1254
DI 10.1109/TGRS.2012.2227760
PN 1
PG 10
WC Geochemistry & Geophysics; Engineering, Electrical & Electronic; Remote
Sensing; Imaging Science & Photographic Technology
SC Geochemistry & Geophysics; Engineering; Remote Sensing; Imaging Science
& Photographic Technology
GA 100TI
UT WOS:000315725900018
ER
PT J
AU Stone, TC
Rossow, WB
Ferrier, J
Hinkelman, LM
AF Stone, Thomas C.
Rossow, William B.
Ferrier, Joseph
Hinkelman, Laura M.
TI Evaluation of ISCCP Multisatellite Radiance Calibration for
Geostationary Imager Visible Channels Using the Moon
SO IEEE TRANSACTIONS ON GEOSCIENCE AND REMOTE SENSING
LA English
DT Article
DE Calibration; Moon; radiometry; remote sensing
ID CLOUD-CLIMATOLOGY-PROJECT; AVHRR; RADIOMETER; SURFACE; PATH
AB Since 1983, the International Satellite Cloud Climatology Project (ISCCP) has collected Earth radiance data from the succession of geostationary and polar-orbiting meteorological satellites operated by weather agencies worldwide. Meeting the ISCCP goals of global coverage and decade-length time scales requires consistent and stable calibration of the participating satellites. For the geostationary imager visible channels, ISCCP calibration provides regular periodic updates from regressions of radiances measured from coincident and collocated observations taken by Advanced Very High Resolution Radiometer instruments. As an independent check of the temporal stability and intersatellite consistency of ISCCP calibrations, we have applied lunar calibration techniques to geostationary imager visible channels using images of the Moon found in the ISCCP data archive. Lunar calibration enables using the reflected light from the Moon as a stable and consistent radiometric reference. Although the technique has general applicability, limitations of the archived image data have restricted the current study to Geostationary Operational Environmental Satellite and Geostationary Meteorological Satellite series. The results of this lunar analysis confirm that ISCCP calibration exhibits negligible temporal trends in sensor response but have revealed apparent relative biases between the satellites at various levels. However, these biases amount to differences of only a few percent in measured absolute reflectances. Since the lunar analysis examines only the lower end of the radiance range, the results suggest that the ISCCP calibration regression approach does not precisely determine the intercept or the zero-radiance response level. We discuss the impact of these findings on the development of consistent calibration for multisatellite global data sets.
C1 [Stone, Thomas C.] US Geol Survey, Astrogeol Sci Ctr, Flagstaff, AZ 86001 USA.
[Rossow, William B.] CUNY, New York, NY 10031 USA.
[Ferrier, Joseph] NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
[Hinkelman, Laura M.] Univ Washington, Joint Inst Study Atmosphere & Ocean, Seattle, WA 98195 USA.
RP Stone, TC (reprint author), US Geol Survey, Astrogeol Sci Ctr, Flagstaff, AZ 86001 USA.
EM tstone@usgs.gov; wbrossow@ccny.cuny.edu; joe@ferrier.com;
laurahin@u.washington.edu
RI Rossow, William/F-3138-2015; Hinkelman, Laura/L-8964-2016
OI Hinkelman, Laura/0000-0001-6477-9648
FU National Aeronautics and Space Administration (NASA) [NNX08AJ80G]; NASA
[NNX08AL79A]
FX This work was supported in part by the National Aeronautics and Space
Administration (NASA) Earth Science Research Program under Interagency
Agreement NNX08AJ80G and in part by the NASA Earth Science Data Systems
Making Earth System Data Records for Use in Research Environments
Program under Contract NNX08AL79A.
NR 19
TC 8
Z9 8
U1 1
U2 6
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 0196-2892
EI 1558-0644
J9 IEEE T GEOSCI REMOTE
JI IEEE Trans. Geosci. Remote Sensing
PD MAR
PY 2013
VL 51
IS 3
SI SI
BP 1255
EP 1266
DI 10.1109/TGRS.2012.2237520
PN 1
PG 12
WC Geochemistry & Geophysics; Engineering, Electrical & Electronic; Remote
Sensing; Imaging Science & Photographic Technology
SC Geochemistry & Geophysics; Engineering; Remote Sensing; Imaging Science
& Photographic Technology
GA 100TI
UT WOS:000315725900019
ER
PT J
AU Chander, G
Mishra, N
Helder, DL
Aaron, DB
Angal, A
Choi, T
Xiong, XX
Doelling, DR
AF Chander, Gyanesh
Mishra, Nischal
Helder, Dennis L.
Aaron, David B.
Angal, Amit
Choi, Taeyoung
Xiong, Xiaoxiong
Doelling, David R.
TI Applications of Spectral Band Adjustment Factors (SBAF) for
Cross-Calibration
SO IEEE TRANSACTIONS ON GEOSCIENCE AND REMOTE SENSING
LA English
DT Article
DE Environmental Satellite (Envisat) Scanning Imaging Absorption
Spectrometer for Atmospheric Cartography (SCIAMACHY); Earth Observing-1
(EO-1) Hyperion; Landsat 7 (L7) Enhanced Thematic Mapper Plus (ETM plus
); radiometric cross-calibration; relative spectral response (RSR);
spectral band adjustment factors (SBAFs); Terra Moderate Resolution
Imaging Spectroradiometer (MODIS)
ID OPTICAL SATELLITE SENSORS; TERRA MODIS; LANDSAT-7 ETM+; PERFORMANCE;
SCIAMACHY; SAHARAN; SITES; TM
AB To monitor land surface processes over a wide range of temporal and spatial scales, it is critical to have coordinated observations of the Earth's surface acquired from multiple space-borne imaging sensors. However, an integrated global observation framework requires an understanding of how land surface processes are seen differently by various sensors. This is particularly true for sensors acquiring data in spectral bands whose relative spectral responses (RSRs) are not similar and thus may produce different results while observing the same target. The intrinsic offsets between two sensors caused by RSR mismatches can be compensated by using a spectral band adjustment factor (SBAF), which takes into account the spectral profile of the target and the RSR of the two sensors. The motivation of this work comes from the need to compensate the spectral response differences of multispectral sensors in order to provide a more accurate cross-calibration between the sensors. In this paper, radiometric cross-calibration of the Landsat 7 Enhanced Thematic Mapper Plus (ETM+) and the Terra Moderate Resolution Imaging Spectroradiometer (MODIS) sensors was performed using near-simultaneous observations over the Libya 4 pseudoinvariant calibration site in the visible and near-infrared spectral range. The RSR differences of the analogous ETM+ and MODIS spectral bands provide the opportunity to explore, understand, quantify, and compensate for the measurement differences between these two sensors. The cross-calibration was initially performed by comparing the top-of-atmosphere (TOA) reflectances between the two sensors over their lifetimes. The average percent differences in the long-term trends ranged from -5% to + 6%. The RSR compensated ETM+ TOA reflectance (ETM+*) measurements were then found to agree with MODIS TOA reflectance to within 5% for all bands when Earth Observing-1 Hyperion hyperspectral data were used to produce the SBAFs. These differences were later reduced to within 1% for all bands (except band 2) by using Environmental Satellite Scanning Imaging Absorption Spectrometer for Atmospheric Cartography hyperspectral data to produce the SBAFs.
C1 [Chander, Gyanesh] US Geol Survey, Stinger Ghaffarian Technol, Earth Resources Observat & Sci EROS Ctr, Sioux Falls, SD 57198 USA.
[Mishra, Nischal; Helder, Dennis L.; Aaron, David B.] S Dakota State Univ, Brookings, SD 57007 USA.
[Angal, Amit] Sci Syst & Applicat Inc, Lanham, MD 20706 USA.
[Choi, Taeyoung] Sigma Space Corp, Lanham, MD 20706 USA.
[Choi, Taeyoung] George Mason Univ, Fairfax, VA 22030 USA.
[Xiong, Xiaoxiong] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Doelling, David R.] NASA, Langley Res Ctr, Hampton, VA 23681 USA.
RP Chander, G (reprint author), US Geol Survey, Stinger Ghaffarian Technol, Earth Resources Observat & Sci EROS Ctr, Sioux Falls, SD 57198 USA.
EM gchander@usgs.gov; Nischal.Mishra@sdstate.edu;
dennis.helder@sdstate.edu; David.Aaron@sdstate.edu;
amit.angal@ssaihq.com; taeyoung.choi@sigmaspace.com;
Xiaoxiong.Xiong-1@nasa.gov; david.r.doelling@nasa.gov
RI Choi, Taeyoung/E-4437-2016; Richards, Amber/K-8203-2015
OI Choi, Taeyoung/0000-0002-4596-989X;
FU National Aeronautics and Space Administration [NNH08AI30I]; U.S.
Geological Survey [G10PC00044]
FX This work was supported in part by the National Aeronautics and Space
Administration Land-Cover and Land-Use Change under Grant NNH08AI30I.
The work of G. Chander was support by the U.S. Geological Survey under
Contract G10PC00044. Any use of trade, product, or firm names is for
descriptive purposes only and does not imply endorsement by the U.S.
Government.
NR 26
TC 34
Z9 36
U1 8
U2 37
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 0196-2892
J9 IEEE T GEOSCI REMOTE
JI IEEE Trans. Geosci. Remote Sensing
PD MAR
PY 2013
VL 51
IS 3
SI SI
BP 1267
EP 1281
DI 10.1109/TGRS.2012.2228007
PN 1
PG 15
WC Geochemistry & Geophysics; Engineering, Electrical & Electronic; Remote
Sensing; Imaging Science & Photographic Technology
SC Geochemistry & Geophysics; Engineering; Remote Sensing; Imaging Science
& Photographic Technology
GA 100TI
UT WOS:000315725900020
ER
PT J
AU Henry, P
Chander, G
Fougnie, B
Thomas, C
Xiong, XX
AF Henry, Patrice
Chander, Gyanesh
Fougnie, Bertrand
Thomas, Colin
Xiong, Xiaoxiong
TI Assessment of Spectral Band Impact on Intercalibration Over Desert Sites
Using Simulation Based on EO-1 Hyperion Data
SO IEEE TRANSACTIONS ON GEOSCIENCE AND REMOTE SENSING
LA English
DT Article
DE Calibration; Envisat MERIS; EO-1 Hyperion; intercalibration; L7 ETM+;
radiometric calibration; reflected solar band; relative spectral
response (RSR); satellites; simulation; Terra and Aqua MODIS
ID OPTICAL SATELLITE SENSORS; IN-FLIGHT CALIBRATION; RADIOMETRIC
CALIBRATION; IMAGING SPECTROMETER; PERFORMANCE; VEGETATION; MERIS;
MODIS; INSTRUMENT; SAHARAN
AB Since the beginning of the 1990s, stable desert sites have been used for the calibration monitoring of many different sensors. Many attempts at sensor intercalibration have been also conducted using these stable desert sites. As a result, site characterization techniques and the quality of intercalibration techniques have gradually improved over the years. More recently, the Committee on Earth Observation Satellites has recommended a list of reference pseudo-invariant calibration sites for frequent image acquisition by multiple agencies. In general, intercalibration should use well-known or spectrally flat reference. The reflectance profile of desert sites, however, might not be flat or well characterized (from a fine spectral point of view). The aim of this paper is to assess the expected accuracy that can be reached when using desert sites for intercalibration. In order to have a well-mastered estimation of different errors or error sources, this study is performed with simulated data from a hyperspectral sensor. Earth Observing-1 Hyperion images are chosen to provide the simulation input data. Two different cases of intercalibration are considered, namely, Landsat 7 Enhanced Thematic Mapper Plus with Terra Moderate Resolution Imaging Spectroradiometer (MODIS) and Environmental Satellite MEdium Resolution Imaging Spectrometer (MERIS) with Aqua MODIS. The simulation results have confirmed that intercalibration accuracy of 1% to 2% can be achieved between sensors, provided there are a sufficient number of available measurements. The simulated intercalibrations allow explaining results obtained during real intercalibration exercises and to establish some recommendations for the use of desert sites for intercalibration.
C1 [Henry, Patrice; Fougnie, Bertrand; Thomas, Colin] Ctr Natl Etud Spatiales, F-31401 Toulouse 9, France.
[Chander, Gyanesh] US Geol Survey, SGT Inc, Earth Resources Observat & Sci EROS Ctr, Sioux Falls, SD 57198 USA.
[Thomas, Colin] CS SI, F-31506 Toulouse 5, France.
[Xiong, Xiaoxiong] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Henry, P (reprint author), Ctr Natl Etud Spatiales, F-31401 Toulouse 9, France.
EM patrice.henry@cnes.fr; gchander@usgs.gov
RI Richards, Amber/K-8203-2015
NR 35
TC 19
Z9 19
U1 0
U2 16
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 0196-2892
J9 IEEE T GEOSCI REMOTE
JI IEEE Trans. Geosci. Remote Sensing
PD MAR
PY 2013
VL 51
IS 3
SI SI
BP 1297
EP 1308
DI 10.1109/TGRS.2012.2228210
PN 1
PG 12
WC Geochemistry & Geophysics; Engineering, Electrical & Electronic; Remote
Sensing; Imaging Science & Photographic Technology
SC Geochemistry & Geophysics; Engineering; Remote Sensing; Imaging Science
& Photographic Technology
GA 100TI
UT WOS:000315725900022
ER
PT J
AU McCorkel, J
Thome, K
Lockwood, RB
AF McCorkel, Joel
Thome, Kurtis
Lockwood, Ronald B.
TI Absolute Radiometric Calibration of Narrow-Swath Imaging Sensors With
Reference to Non-Coincident Wide-Swath Sensors
SO IEEE TRANSACTIONS ON GEOSCIENCE AND REMOTE SENSING
LA English
DT Article
DE Hyperspectral sensors; intercalibration; radiometric calibration;
reflectance retrieval
ID REFLECTANCE-BASED METHOD; CROSS-CALIBRATION; VICARIOUS CALIBRATION;
LANDSAT-7 ETM+; SATELLITE SENSORS; GROUND TARGETS; MODIS; AVHRR;
SPECTROMETER; CHANNELS
AB An inter-calibration method is developed to provide absolute radiometric calibration of narrow-swath imaging sensors with reference to non-coincident wide-swath sensors. The method predicts at-sensor radiance using non-coincident imagery from the reference sensor and knowledge of spectral reflectance of the test site. The imagery of the reference sensor is restricted to acquisitions that provide similar view and solar illumination geometries to reduce uncertainties due to directional reflectance effects. Spectral reflectance of the test site is found with a simple iterative radiative transfer method using radiance values of a well-understood wide-swath sensor and spectral shape information based on historical ground-based measurements. At-sensor radiance is calculated for the narrow-swath sensor using this spectral reflectance and atmospheric parameters that are also based on historical in-situ measurements. Results of the inter-calibration method show agreement on the 2-5% level inmost spectral regions with the vicarious calibration technique relying on coincident ground-based measurements referred to as the reflectance-based approach. While the variability of the inter-calibration method based on non-coincident image pairs is significantly larger, results are consistent with techniques relying on in-situ measurements. The method is also insensitive to spectral differences between the sensors by transferring to surface spectral reflectance prior to prediction of at-sensor radiance. The utility of this inter-calibration method is made clear by its flexibility to utilize image pairings with acquisition dates differing in excess of 30 days allowing frequent absolute calibration comparisons between wideand narrow-swath sensors.
C1 [McCorkel, Joel; Thome, Kurtis] NASA, Goddard Space Flight Ctr, Sci & Explorat Directorate, Greenbelt, MD 20771 USA.
[Lockwood, Ronald B.] MIT, Lincoln Lab, Grp Sensors Technol & Syst Applicat 97, Lexington, MA 02421 USA.
RP McCorkel, J (reprint author), NASA, Goddard Space Flight Ctr, Sci & Explorat Directorate, Greenbelt, MD 20771 USA.
EM joel.mccorkel@gmail.com; kurtis.thome@nasa.gov;
Ronald.lockwood@ll.mit.edu
RI McCorkel, Joel/D-4454-2012; Thome, Kurtis/D-7251-2012
OI McCorkel, Joel/0000-0003-2853-2036;
NR 29
TC 9
Z9 10
U1 1
U2 17
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 0196-2892
J9 IEEE T GEOSCI REMOTE
JI IEEE Trans. Geosci. Remote Sensing
PD MAR
PY 2013
VL 51
IS 3
SI SI
BP 1309
EP 1318
DI 10.1109/TGRS.2012.2219874
PN 1
PG 10
WC Geochemistry & Geophysics; Engineering, Electrical & Electronic; Remote
Sensing; Imaging Science & Photographic Technology
SC Geochemistry & Geophysics; Engineering; Remote Sensing; Imaging Science
& Photographic Technology
GA 100TI
UT WOS:000315725900023
ER
PT J
AU Helder, D
Thome, KJ
Mishra, N
Chander, G
Xiong, XX
Angal, A
Choi, T
AF Helder, Dennis
Thome, Kurtis J.
Mishra, Nischal
Chander, Gyanesh
Xiong, Xiaoxiong
Angal, Amit
Choi, Taeyoung
TI Absolute Radiometric Calibration of Landsat Using a Pseudo Invariant
Calibration Site
SO IEEE TRANSACTIONS ON GEOSCIENCE AND REMOTE SENSING
LA English
DT Article
DE Absolute calibration; EO-1 Hyperion; L7 ETM+; radiometric calibration;
Relative Spectral Response (RSR); Terra MODIS
ID RESOLUTION IMAGING SPECTRORADIOMETER; ON-ORBIT CALIBRATION; VICARIOUS
CALIBRATION; INTEGRATING SPHERE; MODIS; PERFORMANCE; SENSORS; ASTER;
INSTRUMENT; TARGETS
AB Pseudo invariant calibration sites (PICS) have been used for on-orbit radiometric trending of optical satellite systems for more than 15 years. This approach to vicarious calibration has demonstrated a high degree of reliability and repeatability at the level of 1-3% depending on the site, spectral channel, and imaging geometries. A variety of sensors have used this approach for trending because it is broadly applicable and easy to implement. Models to describe the surface reflectance properties, as well as the intervening atmosphere have also been developed to improve the precision of the method. However, one limiting factor of using PICS is that an absolute calibration capability has not yet been fully developed. Because of this, PICS are primarily limited to providing only long term trending information for individual sensors or cross-calibration opportunities between two sensors. This paper builds an argument that PICS can be used more extensively for absolute calibration. To illustrate this, a simple empirical model is developed for the well-known Libya 4 PICS based on observations by Terra MODIS and EO-1 Hyperion. The model is validated by comparing model predicted top-of-atmosphere reflectance values to actual measurements made by the Landsat ETM+ sensor reflective bands. Following this, an outline is presented to develop a more comprehensive and accurate PICS absolute calibration model that can be Systeme international d'unites (SI) traceable. These initial concepts suggest that absolute calibration using PICS is possible on a broad scale and can lead to improved on-orbit calibration capabilities for optical satellite sensors.
C1 [Helder, Dennis; Mishra, Nischal] S Dakota State Univ, Brookings, SD 57007 USA.
[Thome, Kurtis J.; Xiong, Xiaoxiong] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Chander, Gyanesh] US Geol Survey, SGT Inc, Earth Resources Observat & Sci EROS Ctr, Sioux Falls, SD 57198 USA.
[Angal, Amit] Sci Syst & Applicat SSAI Inc, Lanham, MD 20706 USA.
[Choi, Taeyoung] Sigma Space Corp, Lanham, MD 20706 USA.
RP Helder, D (reprint author), S Dakota State Univ, Brookings, SD 57007 USA.
EM Dennis_Helder@sdstate.edu; kurtis.thome@nasa.gov;
Nischal.Mishra@sdstate.edu; gchander@usgs.gov;
xiaoxiong.xiong.1@gsfc.nasa.gov; amit.angal@ssaihq.com;
taeyoung.choi@sigmaspace.com
RI Thome, Kurtis/D-7251-2012; Choi, Taeyoung/E-4437-2016; Richards,
Amber/K-8203-2015
OI Choi, Taeyoung/0000-0002-4596-989X;
FU U.S. Geological Survey [G10PC00044]
FX The work of G. Chander was support by the U.S. Geological Survey under
Contract G10PC00044.
NR 40
TC 27
Z9 28
U1 13
U2 40
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 0196-2892
EI 1558-0644
J9 IEEE T GEOSCI REMOTE
JI IEEE Trans. Geosci. Remote Sensing
PD MAR
PY 2013
VL 51
IS 3
SI SI
BP 1360
EP 1369
DI 10.1109/TGRS.2013.2243738
PN 1
PG 10
WC Geochemistry & Geophysics; Engineering, Electrical & Electronic; Remote
Sensing; Imaging Science & Photographic Technology
SC Geochemistry & Geophysics; Engineering; Remote Sensing; Imaging Science
& Photographic Technology
GA 100TI
UT WOS:000315725900027
ER
PT J
AU Roman, MO
Gatebe, CK
Shuai, YM
Wang, ZS
Gao, F
Masek, JG
He, T
Liang, SL
Schaaf, CB
AF Roman, Miguel O.
Gatebe, Charles K.
Shuai, Yanmin
Wang, Zhuosen
Gao, Feng
Masek, Jeffrey G.
He, Tao
Liang, Shunlin
Schaaf, Crystal B.
TI Use of In Situ and Airborne Multiangle Data to Assess MODIS- and
Landsat-Based Estimates of Directional Reflectance and Albedo
SO IEEE TRANSACTIONS ON GEOSCIENCE AND REMOTE SENSING
LA English
DT Article
DE Biosphere; ecosystems; land surface; remote sensing
ID BIDIRECTIONAL REFLECTANCE; SPECTRAL MEASUREMENTS; SURFACE REFLECTANCE;
BRDF MODELS; RETRIEVALS; VALIDATION; ALGORITHM; RESOLUTION; PRODUCTS;
CONSISTENCY
AB The quantification of uncertainty in satellite-derived global surface albedo products is a critical aspect in producing complete, physically consistent, and decadal land property data records for studying ecosystem change. A challenge in validating albedo measurements acquired from space is the ability to overcome the spatial scaling errors that can produce disagreements between satellite and field-measured values. Here, we present the results from an accuracy assessment of MODIS and Landsat-TM albedo retrievals, based on collocated comparisons with tower and airborne Cloud Absorption Radiometer (CAR) measurements collected during the 2007 Cloud and Land Surface Interaction Campaign (CLASIC). The initial focus was on evaluating inter-sensor consistency through comparisons of intrinsic bidirectional reflectance estimates. Local and regional assessments were then performed to obtain estimates of the resulting scaling uncertainties, and to establish the accuracy of albedo reconstructions during extended periods of precipitation. In general, the satellite-derived estimates met the accuracy requirements established for the high-qualityMODIS operational albedos at 500 m (the greater of 0.02 units or +/- 10% of surface measured values). However, results reveal a high degree of variability in the root-mean-square error (RMSE) and bias of MODIS visible (0.3-0.7 mu m) and Landsat-TM shortwave (0.3-5.0 mu m) albedos; where, in some cases, retrieval uncertainties were found to be in excess of 15%. Results suggest that an overall improvement in MODIS shortwave albedo retrieval accuracy of 7.8%, based on comparisons between MODIS and CAR albedos, resulted from the removal of sub-grid scale mismatch errors when directly scaling-up the tower measurements to the MODIS satellite footprint.
C1 [Roman, Miguel O.; Gatebe, Charles K.; Shuai, Yanmin; Masek, Jeffrey G.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Gatebe, Charles K.] Univ Space Res Assoc, Columbia, MD 21044 USA.
[Shuai, Yanmin] Earth Resources Technol Inc, Laurel, MD 20707 USA.
[Wang, Zhuosen; Schaaf, Crystal B.] Univ Massachusetts, Dept Environm Earth & Ocean Sci, Boston, MA 02125 USA.
[Wang, Zhuosen; Schaaf, Crystal B.] Boston Univ, Ctr Remote Sensing, Dept Geog & Environm, Boston, MA 02215 USA.
[Gao, Feng] ARS, USDA, Hydrol & Remote Sensing Lab, Beltsville, MD 20705 USA.
[He, Tao; Liang, Shunlin] Univ Maryland, Dept Geog Sci, College Pk, MD 20742 USA.
RP Roman, MO (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
EM Miguel.O.Roman@nasa.gov; charles.k.gatebe@nasa.gov;
Yanmin.Shuai@ertcorp.com; wangzhs@bu.edu; Feng.Gao@ars.usda.gov;
jeffrey.g.masek@nasa.gov; the@umd.edu; sliang@umd.edu; schaaf@bu.edu
RI Masek, Jeffrey/D-7673-2012; Gatebe, Charles/G-7094-2011; Roman,
Miguel/D-4764-2012; liang, shunlin/C-2809-2015; He, Tao/H-5130-2012
OI Gatebe, Charles/0000-0001-9261-2239; Roman, Miguel/0000-0003-3953-319X;
He, Tao/0000-0003-2079-7988
FU Science Mission Directorate of the National Aeronautics and Space
Administration as part of the Earth Observing System, Radiation Sciences
Program; Terrestrial Ecology Program; Airborne Sciences Program; NASA
[NNX08AF89G, NNX12AL38G]; U.S. Department of Energy (DOE) Atmospheric
Radiation Measurement (ARM) Program [DOE-DE-FG02-06ER64178]
FX This work was supported by the Science Mission Directorate of the
National Aeronautics and Space Administration as part of the Earth
Observing System, Radiation Sciences Program, the Terrestrial Ecology
Program, and the Airborne Sciences Program. The work of C. K. Gatebe was
supported by NASA Grant NNX08AF89G. The work of C. B. Schaaf was
supported by NASA Grant NNX12AL38G and U.S. Department of Energy (DOE)
Atmospheric Radiation Measurement (ARM) Program under Grant
DOE-DE-FG02-06ER64178.
NR 53
TC 37
Z9 40
U1 3
U2 45
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 0196-2892
EI 1558-0644
J9 IEEE T GEOSCI REMOTE
JI IEEE Trans. Geosci. Remote Sensing
PD MAR
PY 2013
VL 51
IS 3
SI SI
BP 1393
EP 1404
DI 10.1109/TGRS.2013.2243457
PN 1
PG 12
WC Geochemistry & Geophysics; Engineering, Electrical & Electronic; Remote
Sensing; Imaging Science & Photographic Technology
SC Geochemistry & Geophysics; Engineering; Remote Sensing; Imaging Science
& Photographic Technology
GA 100TI
UT WOS:000315725900030
ER
PT J
AU Wu, A
Xiong, X
Angal, A
AF Wu, A.
Xiong, X.
Angal, A.
TI Derive a MODIS-Based Calibration for the AVHRR Reflective Solar Channels
of the NOAA KLM Operational Satellites
SO IEEE TRANSACTIONS ON GEOSCIENCE AND REMOTE SENSING
LA English
DT Article
DE Advanced Very High Resolution Radiometer (AVHRR); bidirectional
reflectance distribution function (BRDF); calibration; desert; Moderate
Resolution Imaging Spectroradiometer (MODIS)
ID SENSOR CALIBRATION; SITES
AB The Advanced Very High Resolution Radiometer (AVHRR) has been on board the National Oceanic and Atmospheric Administration (NOAA) polar-orbiting satellites (POSs) beginning with the Television Infrared Observation Satellite N launched in October 1978. Since then, a series of AVHRR sensors have collected over 30 years of continuous daily global observations. Recently, the NOAA K, L, and M POSs have provided an improved monitoring of the Earth's environment. The AVHRR instrument carried on NOAA-15 (NOAA-K) was launched in May 1998. It is followed by NOAA-16 to NOAA-18 (NOAA-L, NOAA-M, and NOAA-N), Metop-A, and NOAA-19 (NOAA-N'). All of them have been operating to date. An accurate and consistent calibration for the AVHRR reflective solar channels has been challenging as there is no onboard calibrator and vicarious calibration often needs to accumulate large number of reliable observations to derive any meaningful long-term trends. In this paper, we use the Committee on Earth Observation Satellites-endorsed calibration/validation Libya-4 (28.55 N, 23.39 W) desert site to track the long-term stability of reflective solar channels of the NOAA KLM AVHRR. The Moderate Resolution Imaging Spectroradiometer (MODIS) on board the Terra and Aqua platforms is used as a reference to recalibrate the NOAA KLM trends. This study is focused on evaluating the calibration accuracy for the visible and near-infrared channels of each AVHRR instrument using MODIS channels 1 (620-670 nm) and 2 (841-876 nm). A site-specific bidirectional reflectance distribution function developed based on observations made by MODIS is used to normalize AVHRR-observed reflectances. Impacts of atmospheric water vapor on AVHRR-to-MODIS reflectance ratios are corrected with measured total water-vapor contents derived using the split-window temperature difference technique. Finally, MODIS-based AVHRR calibration results, which track the AVHRR on-orbit change, are applied on top of the AVHRR prelaunch values and presented in the form of quadratic polynomials as a function of time. All recalibrated AVHRR reflectances are compared with those provided from a Level 1B product. Additional validation is performed using NOAA-17 AVHRR observations acquired over Antarctic Dome Concordia site where the impact due to atmospheric water vapor is believed to be extremely small.
C1 [Wu, A.] Sigma Space Corp, Lanham, MD 20706 USA.
[Xiong, X.] NASA, Sci & Explorat Directorate, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Angal, A.] Sci Syst & Applicat Inc, Lanham, MD 20706 USA.
RP Wu, A (reprint author), Sigma Space Corp, Lanham, MD 20706 USA.
EM aisheng.wu@sigmaspace.com; Xiaoxiong.Xiong-1@nasa.gov;
amit.angal@ssaihq.com
NR 20
TC 8
Z9 8
U1 1
U2 15
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 0196-2892
J9 IEEE T GEOSCI REMOTE
JI IEEE Trans. Geosci. Remote Sensing
PD MAR
PY 2013
VL 51
IS 3
SI SI
BP 1405
EP 1413
DI 10.1109/TGRS.2012.2220780
PN 1
PG 9
WC Geochemistry & Geophysics; Engineering, Electrical & Electronic; Remote
Sensing; Imaging Science & Photographic Technology
SC Geochemistry & Geophysics; Engineering; Remote Sensing; Imaging Science
& Photographic Technology
GA 100TI
UT WOS:000315725900031
ER
PT J
AU Lukashin, C
Wielicki, BA
Young, DF
Thome, K
Jin, ZH
Sun, WB
AF Lukashin, Constantine
Wielicki, Bruce A.
Young, David F.
Thome, Kurt
Jin, Zhonghai
Sun, Wenbo
TI Uncertainty Estimates for Imager Reference Inter-Calibration With
CLARREO Reflected Solar Spectrometer
SO IEEE TRANSACTIONS ON GEOSCIENCE AND REMOTE SENSING
LA English
DT Article
DE Calibration; polarization; radiometry
ID ANGULAR-DISTRIBUTION MODELS; RADIATIVE FLUX ESTIMATION; ENERGY SYSTEM
INSTRUMENT; PART I; SATELLITE; CLIMATE; PERFORMANCE; METHODOLOGY;
RADIANCE; CLOUDS
AB One of the Climate Absolute Radiance and Refractivity Observatory (CLARREO) mission objectives is to provide a high accuracy calibration standard on orbit to enable intercalibration of existing sensors. In order to perform an accurate inter-calibration of imaging radiometers, such as VIIRS, one must take into account instrument sensitivity to polarization of incoming light. Even if the sensitivity to polarization of an instrument is established or known on orbit, the knowledge of the polarization state of reflected light is required to make relevant radiometric corrections. In the case when coincident polarimetric measurements are not available, we propose to use a combination of empirical and theoretical models to predict the polarization of solar reflected light at the top-of-atmosphere. We used observations from on-orbit polarimeter PARASOL to derive a global set of empirical Polarization Distribution Models (PDM) as a function of scene type and viewing geometry. The PDM accuracy for the mean values is estimated to match the 3% PARASOL uncertainty in its polarization measurements. The instantaneous single sample uncertainty of the prototype PDMs for the linear degree of polarization is contained within 15%. We also present the formalism and numeric estimates for resulting uncertainty for intercalibration of an imaging radiometer with the CLARREO reference observations, including uncertainty due to instrument sensitivity to polarization. The uncertainty estimates consider a range of scenarios with varying data sampling, uncertainty of polarization, and imaging radiometer sensitivity to polarization. These results are used to recommend CLARREO mission requirements relevant to reference inter-calibration and polarization effects.
C1 [Lukashin, Constantine; Wielicki, Bruce A.; Young, David F.] NASA, Langley Res Ctr, Hampton, VA 23681 USA.
[Thome, Kurt] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Jin, Zhonghai; Sun, Wenbo] Sci Syst & Applicat Inc, Hampton, VA 23666 USA.
RP Lukashin, C (reprint author), NASA, Langley Res Ctr, Hampton, VA 23681 USA.
EM Constantine.Lukashin-1@nasa.gov; b.a.wielicki@nasa.gov;
David.F.Young@nasa.gov; kurtis.thome@nasa.gov; zhonghai.jin@nasa.gov;
wenbo.sun-1@nasa.gov
RI Thome, Kurtis/D-7251-2012; Richards, Amber/K-8203-2015
FU NASA CLARREO project
FX This work was supported by the NASA CLARREO project.
NR 26
TC 10
Z9 10
U1 3
U2 13
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 0196-2892
J9 IEEE T GEOSCI REMOTE
JI IEEE Trans. Geosci. Remote Sensing
PD MAR
PY 2013
VL 51
IS 3
SI SI
BP 1425
EP 1436
DI 10.1109/TGRS.2012.2233480
PN 1
PG 12
WC Geochemistry & Geophysics; Engineering, Electrical & Electronic; Remote
Sensing; Imaging Science & Photographic Technology
SC Geochemistry & Geophysics; Engineering; Remote Sensing; Imaging Science
& Photographic Technology
GA 100TI
UT WOS:000315725900033
ER
PT J
AU Biswas, SK
Farrar, S
Gopalan, K
Santos-Garcia, A
Jones, WL
Bilanow, S
AF Biswas, Sayak K.
Farrar, Spencer
Gopalan, Kaushik
Santos-Garcia, Andrea
Jones, W. Linwood
Bilanow, Stephen
TI Intercalibration of Microwave Radiometer Brightness Temperatures for the
Global Precipitation Measurement Mission
SO IEEE TRANSACTIONS ON GEOSCIENCE AND REMOTE SENSING
LA English
DT Article
DE Global Precipitation Measurement (GPM) Intersatellite Radiometer
Calibration Working Group (XCAL); intersatellite radiometric
calibration; microwave radiometry
ID SATELLITE-OBSERVATIONS; CALIBRATION; SURFACE; WINDSAT; MODEL; WATER;
PERFORMANCE; FREQUENCIES; EMISSIVITY; IMAGER
AB A technique for comparing spaceborne microwave radiometer brightness temperatures (Tb) is described in the context of the upcoming National Aeronautics and Space Administration Global Precipitation Measurement (GPM) mission. The GPM mission strategy is to measure precipitation globally with high temporal resolution by using a constellation of satellite radiometers logically united by the GPM core satellite, which will be in a non-sun-synchronous medium inclination orbit. The usefulness of the combined product depends on the consistency of precipitation retrievals from the various microwave radiometers. The Tb calibration requirement to achieve such consistency demands first that Tb's from the individual radiometers be free of instrument and measurement artifacts and, second, that these self-consistent Tb's will be translated to a common standard (GPM core) for the unification of the precipitation retrieval. The intersatellite radiometric calibration technique described herein serves both the purposes by comparing individual radiometer observations to radiative transfer model (RTM) simulations (for "self-consistency" check) and by using a double-difference technique (to establish a linear calibration transfer function from one radiometer to another). This double-difference technique subtracts the RTM-simulated difference from the observed difference between a pair of radiometer Tb's. To establish a linear inter-radiometer calibration transfer function, comparisons at both the cold (ocean) and the warm (land) end of the Tb's are necessary so that, using these two points, slope and offset coefficients are determined. To this end, a simplified calibration transfer technique at the warm end (over the Amazon and Congo rain forest) is introduced. Finally, an error model is described that provides an estimate of the uncertainty of the radiometric bias estimate between comparison radiometer channels.
C1 [Biswas, Sayak K.; Farrar, Spencer; Gopalan, Kaushik; Santos-Garcia, Andrea; Jones, W. Linwood] Univ Cent Florida, Sch Elect Engn & Comp Sci, Orlando, FL 32816 USA.
[Gopalan, Kaushik] Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20740 USA.
[Bilanow, Stephen] Wyle Informat Syst, Mclean, VA 22102 USA.
RP Biswas, SK (reprint author), NASA, Marshall Space Flight Ctr, Huntsville, AL 35805 USA.
EM sayak.k.biswas@nasa.gov; zepplin_32169@yahoo.com; kaubega@gmail.com;
asantosgarcia@gmail.com; ljones5@cfl.rr.com; stephen.bilanow-1@nasa.gov
RI Measurement, Global/C-4698-2015;
OI Gopalan, Kaushik/0000-0002-7980-6183
FU National Aeronautics and Space Administration Headquarters Earth
Sciences Division
FX This work was supported by a National Aeronautics and Space
Administration Headquarters Earth Sciences Division grant for the
Precipitation Measurement Mission science team.
NR 40
TC 22
Z9 22
U1 1
U2 15
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 0196-2892
J9 IEEE T GEOSCI REMOTE
JI IEEE Trans. Geosci. Remote Sensing
PD MAR
PY 2013
VL 51
IS 3
SI SI
BP 1465
EP 1477
DI 10.1109/TGRS.2012.2217148
PN 1
PG 13
WC Geochemistry & Geophysics; Engineering, Electrical & Electronic; Remote
Sensing; Imaging Science & Photographic Technology
SC Geochemistry & Geophysics; Engineering; Remote Sensing; Imaging Science
& Photographic Technology
GA 100TI
UT WOS:000315725900036
ER
PT J
AU Brown, S
AF Brown, Shannon
TI Maintaining the Long-Term Calibration of the Jason-2/OSTM Advanced
Microwave Radiometer Through Intersatellite Calibration
SO IEEE TRANSACTIONS ON GEOSCIENCE AND REMOTE SENSING
LA English
DT Article
DE Advanced Microwave Scanning Radiometer for EOS (AMSR-E); intersatellite
calibration; Jason-1; Jason-2/Ocean Surface Topography Mission (OSTM);
microwave radiometer; path delay (PD); satellite altimetry; Special
Sensor Microwave Imager/Sounder (SSMIS); Tropical Rainfall Measuring
Mission (TRMM) Microwave Imager (TMI)
ID VICARIOUS COLD REFERENCE; IN-FLIGHT CALIBRATION; ON-ORBIT CALIBRATION;
STABILITY; TOPEX; WINDSAT; MISSION; SSM/I; WATER
AB A method is applied to maintain the long-term calibration of a microwave radiometer through intersatellite calibration and is used to mitigate an observed calibration drift of the Advanced Microwave Radiometer (AMR) on Jason-2/Ocean Surface Topography Mission. The AMR provides a correction for the wet tropospheric path delay (PD) of the radar altimeter signal, and it is critical that any drift in the radiometer be estimated and removed to enable studies of global mean sea-level variability. The intersatellite calibration method transfers the long-term calibration from other satellite microwave radiometers using a transfer function to map the other sensor's brightness temperature (TB) observations to those of the AMR. Intersensor mapping functions are derived separately for ocean observations and observations over the Amazon rainforest. This provides a warm and cold TB calibration reference to enable the distinction between long-term gain and offset drifts. A database of co-incident observations is generated between the AMR and conically scanning microwave sensors, namely, AMSR-E, TMI, and SSMIS. Monthly averaged differences are found between the AMR and the AMR equivalent TBs computed from the reference sensors. The apparent change in the AMR calibration determined from the three reference sensors is intercompared between the sensors and compared to that determined using natural on-Earth references. It is found that apparent trends in the AMR TBs between the reference sensors and the natural on-Earth references agree within amonth to better than 0.4 K. The AMR 18.7- and 23.8-GHz channels are found to be stable to 0.5 K over the first three years of the mission, and the calibration 34.0-GHz channel is found to drift downward by approximately 6 K. In all channels, the calibration change is determined to be a series of offset jumps (independent of TB). These calibration changes in each AMR channel are estimated and removed using the comparisons to the reference sensors. The uncertainty in the PD long-term stability after recalibration is estimated to be less than 0.5 mm/year from July 2008 to August 2011.
C1 CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
RP Brown, S (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91125 USA.
EM Shannon.T.Brown@jpl.nasa.gov
NR 24
TC 9
Z9 9
U1 1
U2 30
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 0196-2892
EI 1558-0644
J9 IEEE T GEOSCI REMOTE
JI IEEE Trans. Geosci. Remote Sensing
PD MAR
PY 2013
VL 51
IS 3
SI SI
BP 1531
EP 1543
DI 10.1109/TGRS.2012.2213262
PN 1
PG 13
WC Geochemistry & Geophysics; Engineering, Electrical & Electronic; Remote
Sensing; Imaging Science & Photographic Technology
SC Geochemistry & Geophysics; Engineering; Remote Sensing; Imaging Science
& Photographic Technology
GA 100TI
UT WOS:000315725900041
ER
PT J
AU Kohler, J
Neumann, TA
Robbins, JW
Tronstad, S
Melland, G
AF Kohler, Jack
Neumann, Thomas A.
Robbins, John W.
Tronstad, Stein
Melland, Gudmund
TI ICESat Elevations in Antarctica Along the 2007-09 Norway-USA Traverse:
Validation With Ground-Based GPS
SO IEEE TRANSACTIONS ON GEOSCIENCE AND REMOTE SENSING
LA English
DT Article
DE Altimetry; ice; laser measurements; radar altimetry; remote sensing
ID SATELLITE RADAR; LASER
AB The 2007-09 Norway-USA Traverse of East Antarctica collected dual-frequency Global Positioning System (GPS) data at 5-s intervals on two of the traverse vehicles. The traverse covered 2400 km from the coast to the vicinity of the Amundsen-Scott South Pole Station in 2007-08, and a 2600 km route from the South Pole to the coast in 2008-09. Side traverses were also conducted in 2008-09, for a total of over 10 000 km of GPS data between the two vehicles. We use precise point positioning to post-process our single receiver kinematic GPS data. Analysis of data obtained while the vehicles were stationary shows individual solutions are accurate to ca. 1 cm horizontally and 3 cm vertically. We compare our GPS elevations with those determined by the National Aeronautics and Space Administration's Ice, Cloud, and Land Elevation Satellite (ICESat), a space-based altimeter designed to measure ice elevation. ICESat accuracy is evaluated by cross-over analysis; mean differences calculated between dh/dt-corrected ICESat data and GPS-derived surface elevations for two vehicles and two traverse seasons range from -12 to -2 cm, within ICESat's stated goal of +/- 15 cm, while 1-sigma values of the same data imply that ICESat's precision is ca. 15.8 cm.
C1 [Kohler, Jack] Norwegian Polar Res Inst, Res Dept, N-9296 Tromso, Norway.
[Neumann, Thomas A.; Robbins, John W.] NASA Goddard Space Flight Ctr, Cryospher Sci Branch, Greenbelt, MD 20770 USA.
[Tronstad, Stein; Melland, Gudmund] Norwegian Polar Res Inst, Environm Management Dept, N-9296 Tromso, Norway.
[Melland, Gudmund] TerraTec AS, N-7434 Trondheim, Norway.
RP Kohler, J (reprint author), Norwegian Polar Res Inst, Res Dept, N-9296 Tromso, Norway.
EM jack.kohler@npolar.no; thomas.Neumann@nasa.gov; john.w.robbins@nasa.gov;
stein.tronstad@npolar.no; gudmund.melland@terratec.no
RI Neumann, Thomas/D-5264-2012
FU Norwegian Polar Institute [152]; Research Council of Norway; US National
Science Foundation
FX Manuscript received July 25, 2011; revised February 27, 2012; accepted
May 15, 2012. Date of publication September 13, 2012; date of current
version February 21, 2013. This work has been carried out under the
umbrella of TASTE-IDEA within the framework of IPY project 152 funded by
Norwegian Polar Institute, the Research Council of Norway, and the US
National Science Foundation.
NR 23
TC 4
Z9 4
U1 1
U2 19
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 0196-2892
EI 1558-0644
J9 IEEE T GEOSCI REMOTE
JI IEEE Trans. Geosci. Remote Sensing
PD MAR
PY 2013
VL 51
IS 3
BP 1578
EP 1587
DI 10.1109/TGRS.2012.2207963
PN 2
PG 10
WC Geochemistry & Geophysics; Engineering, Electrical & Electronic; Remote
Sensing; Imaging Science & Photographic Technology
SC Geochemistry & Geophysics; Engineering; Remote Sensing; Imaging Science
& Photographic Technology
GA 100TJ
UT WOS:000315726100004
ER
PT J
AU Mladenova, IE
Jackson, TJ
Bindlish, R
Hensley, S
AF Mladenova, Iliana E.
Jackson, Thomas J.
Bindlish, Rajat
Hensley, Scott
TI Incidence Angle Normalization of Radar Backscatter Data
SO IEEE TRANSACTIONS ON GEOSCIENCE AND REMOTE SENSING
LA English
DT Article
DE Backscatter; incidence angle effect; incidence angle normalization; Soil
Moisture Active Passive (SMAP)
ID SURFACE SOIL-MOISTURE; BOREAL FOREST; AIRSAR DATA; ASAR DATA; IMAGES;
MODEL; CLASSIFICATION; PERFORMANCE; CANADA; SENSOR
AB The National Aeronautics and Space Administration's (NASA) proposed Soil Moisture Active Passive (SMAP) satellite mission (similar to 2014) will include a radar system that will provide L-band multi-polarization backscatter at a constant incidence angle of 40 degrees. During the pre-launch phase of the project, there is a need for observations that will support the radar-based soil moisture algorithm development and validation. A valuable resource for providing these observations is the NASA Jet Propulsion Laboratory Uninhabited Aerial Vehicle Synthetic Aperture Radar (UAVSAR). However, SMAP will observe at a constant incidence angle of 40 degrees, and UAVSAR collects data over a wide range of incidence angles (25 degrees-60 degrees). In this investigation, a technique was developed and tested for normalizing UAVSAR data to a constant incidence angle. The approach is based on a histogram matching procedure. The data used to develop and demonstrate this approach were collected as part of the Canadian Soil Moisture Experiment 2010 (CanEx-SM10). Land cover in the region included agriculture and forest. Evaluation was made possible by the acquisition of numerous overlapping UAVSAR flight lines that provided multiple incidence angle observations of the same locations. Actual observations at a 40 degrees incidence angle were compared to the normalized data to assess performance of the normalization technique. An optimum technique should be able to reduce the systematic error (Bias) to 0 dB and to lower the total root mean square error (RMSE) computed after correction to the level of the initial residual error (RMSEres) present in the data set. The normalization approach developed here achieved both of these. Bias caused by the incidence angle variability was minimized to similar to 0 dB, whereas the residual error caused by instrument related random errors and amplitude fluctuations due to ground variability was reduced to approximately 3 dB for agricultural areas and 2.6 dB for forests; these values were consistent with the initial RMSEres estimated using the un-corrected data. The residual error can be reduced further by aggregating the radar observations to a coarser grid spacing. The technique adequately adjusted the backscatter over the full swath width irrespective of the original incidence angle, polarization, and ground conditions (vegetation cover and soil moisture). In addition to providing a basis for fully exploiting UAVSAR (or similar aircraft systems) for SMAP algorithm development and validation, the technique could also be adapted to satellite radar systems. This normalization approach will also be beneficial in terms of reducing the number of flight lines required to cover a study area, which would eventually result in more cost-effective soil moisture field campaigns.
C1 [Mladenova, Iliana E.; Jackson, Thomas J.] USDA, Hydrol & Remote Sensing Lab, Beltsville, MD 20740 USA.
[Bindlish, Rajat] Sci Syst & Applicat Inc, Lanham, MD 20706 USA.
[Hensley, Scott] NASA, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Mladenova, IE (reprint author), USDA, Hydrol & Remote Sensing Lab, Beltsville, MD 20740 USA.
EM Iliana.Mladenova@ars.usda.gov; thomas.jackson@ars.usda.gov;
rajat.bindlish@ars.usda.gov; scott.hensley@jpl.nasa.gov
NR 38
TC 15
Z9 15
U1 1
U2 24
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 0196-2892
J9 IEEE T GEOSCI REMOTE
JI IEEE Trans. Geosci. Remote Sensing
PD MAR
PY 2013
VL 51
IS 3
BP 1791
EP 1804
DI 10.1109/TGRS.2012.2205264
PN 2
PG 14
WC Geochemistry & Geophysics; Engineering, Electrical & Electronic; Remote
Sensing; Imaging Science & Photographic Technology
SC Geochemistry & Geophysics; Engineering; Remote Sensing; Imaging Science
& Photographic Technology
GA 100TJ
UT WOS:000315726100021
ER
PT J
AU Gabb, TP
Gayda, J
Telesman, J
Ghosn, LJ
Garg, A
AF Gabb, T. P.
Gayda, J.
Telesman, J.
Ghosn, L. J.
Garg, A.
TI Factors influencing dwell fatigue life in notches of a powder metallurgy
superalloy
SO INTERNATIONAL JOURNAL OF FATIGUE
LA English
DT Article; Proceedings Paper
CT 19th European Conference on Fracture (ECF19)
CY AUG 26-31, 2012
CL Kazan, RUSSIA
SP Russian Acad Sci, Kazan Sci Ctr
DE Superalloy; Disk; Notch; Fatigue; Dwells
ID MICROSTRUCTURE
AB The influences of heat treatment and cyclic dwells on the notch fatigue resistance of powder metallurgy disk superalloys were investigated for the LSHR disk superalloy. Disks were processed to produce material conditions with varied microstructures and associated mechanical properties. Notched specimens were subjected to fatigue cycles having a dwell at maximum load, as well as tensile, stress relaxation, creep rupture, and dwell fatigue crack growth tests at 704 degrees C. Two material conditions displayed a wide distribution of fatigue lives, with low lives reduced by two orders of magnitude, while others had more consistent fatigue lives. The occurrence of these very low lives was compared to other mechanical properties, in search of correlations. The low life failures for dwell fatigue life were correlated with material conditions giving highest ultimate tensile strengths and stress relaxation resistance. These results were analyzed by modeling relaxation of peak stresses in the notch with continued dwell fatigue cycling. Published by Elsevier Ltd.
C1 [Gabb, T. P.; Gayda, J.; Telesman, J.; Ghosn, L. J.] NASA Glenn Res Ctr, Cleveland, OH 44135 USA.
[Garg, A.] Univ Toledo, Toledo, OH 43606 USA.
RP Gabb, TP (reprint author), NASA Glenn Res Ctr, Cleveland, OH 44135 USA.
EM tim.gabb@grc.nasa.gov
FU NASA
FX The authors wish to acknowledge the support of the NASA Aviation Safety
and Vehicle Systems Safety Technologies programs. The assistance of Ron
Jaworsky on fractography is also appreciated. LSHR powder atomization
was performed at PCC Special Metals Corp. under the direction of Tony
Banik, now at Allvac ATI. LSHR disk forging and heat treatments were
performed at PCC Wyman-Gordon Forgings under the direction of Ian
Dempster. David Mourer of GE Aviation and Mark Hardy of Rolls-Royce are
acknowledged for very helpful technical discussions during the work. The
authors also gratefully acknowledge the manuscript improvements
suggested by the journal's reviewers.
NR 17
TC 5
Z9 6
U1 0
U2 12
PU ELSEVIER SCI LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND
SN 0142-1123
EI 1879-3452
J9 INT J FATIGUE
JI Int. J. Fatigue
PD MAR
PY 2013
VL 48
BP 55
EP 67
DI 10.1016/j.ijfatigue.2012.10.003
PG 13
WC Engineering, Mechanical; Materials Science, Multidisciplinary
SC Engineering; Materials Science
GA 099JO
UT WOS:000315617500008
ER
PT J
AU Comarazamy, DE
Gonzalez, JE
Luvall, JC
Rickman, DL
Bornstein, RD
AF Comarazamy, Daniel E.
Gonzalez, Jorge E.
Luvall, Jeffrey C.
Rickman, Douglas L.
Bornstein, Robert D.
TI Climate Impacts of Land-Cover and Land-Use Changes in Tropical Islands
under Conditions of Global Climate Change
SO JOURNAL OF CLIMATE
LA English
DT Article
ID URBAN HEAT-ISLAND; PUERTO-RICO; CARIBBEAN RAINFALL; FIELD SIGNIFICANCE;
SAN-JUAN; MODEL; PRECIPITATION; CONSERVATION; SIMULATION; ATLANTIC
AB Land-cover and land-use (LCLU) changes have significant climate impacts in tropical coastal regions with the added complexity of occurring within the context of a warming climate. The individual and combined effects of these two factors in tropical islands are investigated by use of an integrated mesoscale atmospheric modeling approach, taking the northeastern region of Puerto Rico as the test case. To achieve this goal, an ensemble of climate simulations is performed, combining two LCLU and global warming scenarios. Reconstructed agricultural maps and sea surface temperatures form the past (1955-59) scenario, while the present (2000-04) scenario is supported with high-resolution remote sensing LCLU data. Here, the authors show that LCLU changes produced the largest near-surface (2-m AGL) air temperature differences over heavily urbanized regions and that these changes do not penetrate the boundary layer. The influence of the global warming signal induces a positive inland gradient of maximum temperature, possibly because of increased trade winds in the present climatology. These increased winds also generate convergence zones and convection that transport heat and moisture into the boundary layer. In terms of minimum temperatures, the global warming signal induces temperature increases along the coastal plains and inland lowlands.
C1 [Comarazamy, Daniel E.] CUNY City Coll, NOAA, CREST Ctr, New York, NY 10031 USA.
[Gonzalez, Jorge E.] CUNY City Coll, NOAA, Cooperat Remote Sensing Sci & Technol Ctr CREST, New York, NY 10031 USA.
[Gonzalez, Jorge E.] CUNY City Coll, Dept Mech Engn, New York, NY 10031 USA.
[Luvall, Jeffrey C.; Rickman, Douglas L.] NASA, Global Hydrol & Climate Ctr, Marshall Space Flight Ctr, Huntsville, AL USA.
[Bornstein, Robert D.] San Jose State Univ, Dept Meteorol & Climate, San Jose, CA 95192 USA.
RP Comarazamy, DE (reprint author), NOAA, CREST, T-107,Steinman Hall,140th St & Convent Ave, New York, NY 10031 USA.
EM dcomarazamy@ccny.cuny.edu
RI Comarazamy, Daniel/C-8246-2014;
OI Rickman, Doug/0000-0003-3409-2882
FU NOAA/Cooperative Remote Sensing Science and Technology Center (CREST)
[NA06OAR4810162]
FX This research was funded by NOAA/Cooperative Remote Sensing Science and
Technology Center (CREST) Grant NA06OAR4810162. The atmospheric model
simulations were performed at the High Performance Computing Facilities
of the University of Puerto Rico at Rio Piedras.
NR 50
TC 14
Z9 14
U1 2
U2 59
PU AMER METEOROLOGICAL SOC
PI BOSTON
PA 45 BEACON ST, BOSTON, MA 02108-3693 USA
SN 0894-8755
J9 J CLIMATE
JI J. Clim.
PD MAR
PY 2013
VL 26
IS 5
BP 1535
EP 1550
DI 10.1175/JCLI-D-12-00087.1
PG 16
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 098TK
UT WOS:000315571800005
ER
PT J
AU Shiri, S
Wasylkiwskyj, W
AF Shiri, Shahram
Wasylkiwskyj, Wasyl
TI Poisson-spot intensity reduction with a partially transparent
petal-shaped optical mask
SO JOURNAL OF OPTICS
LA English
DT Article
DE Poisson spot; Arago spot; diffraction; intensity suppression; apodized
petaled mask
AB The presence of a Poisson spot inside a shadow region can best be described as the consequence of constructive interference of light waves diffracted on the edge of the obstruction where its central position can be determined by the symmetry of the object. More recently, the elimination of this spot has received attention in the fields of particle physics, high-energy lasers, astronomy, and lithography. The desired level of intensity suppression is dependent on the type of light source and the field of application. In this paper, we introduce a novel, partially transparent petaled mask shape that suppresses the bright spot by up to ten orders of magnitude in intensity at optical ranges, with potential powerful applications in many of the above fields. The optimization technique formulated in this design can identify mask shapes having partial transparency only near the petal tips.
C1 [Shiri, Shahram] NASA, Goddard Space Flight Ctr, Opt Branch, Greenbelt, MD 20771 USA.
[Wasylkiwskyj, Wasyl] George Washington Univ, Elect & Comp Engn Dept, Washington, DC 20037 USA.
RP Shiri, S (reprint author), NASA, Goddard Space Flight Ctr, Opt Branch, Greenbelt, MD 20771 USA.
EM ron.shiri@nasa.gov
NR 16
TC 4
Z9 4
U1 0
U2 3
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 2040-8978
J9 J OPTICS-UK
JI J. Opt.
PD MAR
PY 2013
VL 15
IS 3
AR 035705
DI 10.1088/2040-8978/15/3/035705
PG 6
WC Optics
SC Optics
GA 099AK
UT WOS:000315590700031
ER
PT J
AU Aquila, V
Oman, LD
Stolarski, R
Douglass, AR
Newman, PA
AF Aquila, V.
Oman, L. D.
Stolarski, R.
Douglass, A. R.
Newman, P. A.
TI The Response of Ozone and Nitrogen Dioxide to the Eruption of Mt.
Pinatubo at Southern and Northern Midlatitudes
SO JOURNAL OF THE ATMOSPHERIC SCIENCES
LA English
DT Article
ID MOUNT-PINATUBO; STRATOSPHERIC OZONE; VOLCANIC-ERUPTIONS; AEROSOL
VARIATIONS; SULFATE AEROSOLS; IN-SITU; DEPLETION; CLIMATE; NO2; TRENDS
AB Observations have shown that the mass of nitrogen dioxide decreased at both southern and northern midlatitudes in the year following the eruption of Mt. Pinatubo, indicating that the volcanic aerosol had enhanced nitrogen dioxide depletion via heterogeneous chemistry. In contrast, the observed ozone response showed a northern midlatitude decrease and a small southern midlatitude increase. Previous simulations that included an enhancement of heterogeneous chemistry by the volcanic aerosol but no other effect of this aerosol produce ozone decreases in both hemispheres, contrary to observations. The authors' simulations show that the heating due to the volcanic aerosol enhanced both the tropical upwelling and Southern Hemisphere extratropical downwelling. This enhanced extratropical downwelling, combined with the time of the eruption relative to the phase of the Brewer-Dobson circulation, increased Southern Hemisphere ozone via advection, counteracting the ozone depletion due to heterogeneous chemistry on the Pinatubo aerosol.
C1 [Aquila, V.; Oman, L. D.; Stolarski, R.; Douglass, A. R.; Newman, P. A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Stolarski, R.] Johns Hopkins Univ, Dept Earth & Planetary Sci, Baltimore, MD 21218 USA.
RP Aquila, V (reprint author), NASA, Goddard Space Flight Ctr, Code 614, Greenbelt, MD 20771 USA.
EM valentina.aquila@nasa.gov
RI Stolarski, Richard/B-8499-2013; Aquila, Valentina/D-7267-2012; Douglass,
Anne/D-4655-2012; Oman, Luke/C-2778-2009; Newman, Paul/D-6208-2012
OI Stolarski, Richard/0000-0001-8722-4012; Aquila,
Valentina/0000-0003-2060-6694; Oman, Luke/0000-0002-5487-2598; Newman,
Paul/0000-0003-1139-2508
FU GOCART; Eric Nash; TOMS
FX We thank Peter Colarco for support with GOCART, Eric Nash for
programming support, Stacey Frith for support with TOMS and SAGE-II
data, and three anonymous reviewers for their useful comments. V. Aquila
is supported by the NASA Post-doctoral Program, administered by the Oak
Ridge Associated University (ORAU). This research was supported by the
NASA MAP program. Our simulations where performed on the Pleiades
supercomputer, administered by the NASA Advance Supercomputing Division
through the NASA High-End Computing Program.
NR 44
TC 23
Z9 24
U1 1
U2 30
PU AMER METEOROLOGICAL SOC
PI BOSTON
PA 45 BEACON ST, BOSTON, MA 02108-3693 USA
SN 0022-4928
J9 J ATMOS SCI
JI J. Atmos. Sci.
PD MAR
PY 2013
VL 70
IS 3
BP 894
EP 900
DI 10.1175/JAS-D-12-0143.1
PG 7
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 101YW
UT WOS:000315811300010
ER
PT J
AU Marsili, F
Verma, VB
Stern, JA
Harrington, S
Lita, AE
Gerrits, T
Vayshenker, I
Baek, B
Shaw, MD
Mirin, RP
Nam, SW
AF Marsili, F.
Verma, V. B.
Stern, J. A.
Harrington, S.
Lita, A. E.
Gerrits, T.
Vayshenker, I.
Baek, B.
Shaw, M. D.
Mirin, R. P.
Nam, S. W.
TI Detecting single infrared photons with 93% system efficiency
SO NATURE PHOTONICS
LA English
DT Article
AB Single-photon detectors(1) at near-infrared wavelengths with high system detection efficiency (>90%), low dark count rate (<1 c.p.s.), low timing jitter (<100 ps) and short reset time (<100 ns) would enable landmark experiments in a variety of fields(2-6). Although some of the existing approaches to single-photon detection fulfil one or two of the above specifications(1), to date, no detector has met all of the specifications simultaneously. Here, we report on a fibre-coupled single-photon detection system that uses superconducting nanowire single-photon detector(7) and closely approaches the ideal performance of single-photon detectors. Our detector system has a system detection efficiency (including optical coupling losses) greater than 90% in the wavelength range lambda = 1,520-1,610 nm, with a device dark count rate (measured with the device shielded from any background radiation) of similar to 1 c.p.s., timing jitter of similar to 150 ps full-width at half-maximum (FWHM) and reset time of 40 ns.
C1 [Marsili, F.; Verma, V. B.; Harrington, S.; Lita, A. E.; Gerrits, T.; Vayshenker, I.; Baek, B.; Mirin, R. P.; Nam, S. W.] NIST, Boulder, CO 80305 USA.
[Stern, J. A.; Shaw, M. D.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Marsili, F (reprint author), NIST, 325 Broadway,MC 815-04, Boulder, CO 80305 USA.
EM francesco.marsili@nist.gov; saewoo.nam@nist.gov
RI Vayshenker, Igor/H-9793-2013;
OI Vayshenker, Igor/0000-0002-7098-3781; Mirin, Richard/0000-0002-4472-4655
FU Defense Advanced Research Projects Agency; National Aeronautics and
Space Administration
FX The authors thank R. M. Briggs, S. D. Dyer, W. H. Farr, J. Gao, M.
Green, E. Grossman, P. D. Hale, R. W. Leonhardt, I. Levin and R. E.
Muller for technical support, and S. Bradley, B. Calkins, A. Migdall and
M. Stevens for scientific discussions. Part of this work was supported
by the Defense Advanced Research Projects Agency (Information in a
Photon programme). Part of this research was carried out at the Jet
Propulsion Laboratory, California Institute of Technology, under a
contract with the National Aeronautics and Space Administration.
NR 30
TC 341
Z9 347
U1 13
U2 123
PU NATURE PUBLISHING GROUP
PI LONDON
PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND
SN 1749-4885
J9 NAT PHOTONICS
JI Nat. Photonics
PD MAR
PY 2013
VL 7
IS 3
BP 210
EP 214
DI 10.1038/NPHOTON.2013.13
PG 5
WC Optics; Physics, Applied
SC Optics; Physics
GA 106OP
UT WOS:000316154700014
ER
PT J
AU Werneth, CM
Norbury, JW
Blattnig, SR
AF Werneth, Charles M.
Norbury, John W.
Blattnig, Steve R.
TI Pion cross section parameterizations for space radiation codes
SO NUCLEAR INSTRUMENTS & METHODS IN PHYSICS RESEARCH SECTION B-BEAM
INTERACTIONS WITH MATERIALS AND ATOMS
LA English
DT Article
DE Inclusive pion cross sections; Badhwar model; Thermal model
ID HEAVY-ION COLLISIONS; QUANTUM MOLECULAR-DYNAMICS; ENERGY NUCLEAR
COLLISIONS; MONTE-CARLO CALCULATIONS; PARTICLE-PRODUCTION; FIREBALL
MODEL; PROTON-PROTON; INTRANUCLEAR CASCADES; FIRESTREAK MODEL; LIGHT
FRAGMENTS
AB The space radiation environment consists of energetic particles that originate from the Sun and from sources outside the solar system. It is necessary to understand how these particles interact with materials to design effective radiation shielding. The transport of radiation through materials can be described by the Boltzmann equation. Efficient space radiation transport codes often require parameterized energy-dependent spectral distributions. A recent study showed that pions may contribute considerably to the total dose in galactic cosmic ray environments. Consequently, accurate parameterized pion spectral distributions are needed. In other studies, the Badhwar parameterization has been used for inclusive pion production in high energy nucleon-nucleon and nucleon-nucleus collisions, whereas a thermal model has been used to describe pion production in low energy nuclear collisions. In this paper, the thermal model is parameterized in terms of projectile energy, projectile nucleon number, and target nucleon number. Thermal and Badhwar model predictions of pion spectra from nucleon-nucleus and nucleus-nucleus collisions are compared for projectile energies ranging from 0.3 to 158 A GeV. It is recommended that the thermal model be used for projectile energies between 0.4 and 5 A GeV and the Badhwar model be used for higher projectile energies. Published by Elsevier B.V.
C1 [Werneth, Charles M.] Univ Tennessee, Dept Nucl Engn, Knoxville, TN 37996 USA.
[Norbury, John W.; Blattnig, Steve R.] NASA, Langley Res Ctr, Hampton, VA 23681 USA.
RP Werneth, CM (reprint author), Univ Tennessee, Dept Nucl Engn, 315 Pasqua Engn Bldg, Knoxville, TN 37996 USA.
EM cwerneth@utk.edu; John.W.Norbury@nasa.gov; Steve.R.Blattnig@nasa.gov
FU NASA [NNX10AD18A]
FX The authors thank Drs. Ryan Norman, Anne Adamczyk, Francis Badavi, and
Jonathan Ransom for reviewing this paper. This work was supported in
part by NASA Grant NNX10AD18A.
NR 58
TC 0
Z9 0
U1 0
U2 2
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0168-583X
J9 NUCL INSTRUM METH B
JI Nucl. Instrum. Methods Phys. Res. Sect. B-Beam Interact. Mater. Atoms
PD MAR 1
PY 2013
VL 298
BP 86
EP 95
DI 10.1016/j.nimb.2012.12.121
PG 10
WC Instruments & Instrumentation; Nuclear Science & Technology; Physics,
Atomic, Molecular & Chemical; Physics, Nuclear
SC Instruments & Instrumentation; Nuclear Science & Technology; Physics
GA 105CM
UT WOS:000316043200014
ER
PT J
AU Fauvel, M
Tarabalka, Y
Benediktsson, JA
Chanussot, J
Tilton, JC
AF Fauvel, Mathieu
Tarabalka, Yuliya
Benediktsson, Jon Atli
Chanussot, Jocelyn
Tilton, James C.
TI Advances in Spectral-Spatial Classification of Hyperspectral Images
SO PROCEEDINGS OF THE IEEE
LA English
DT Article
DE Classification; hyperspectral image; kernel methods; mathematical
morphology; morphological neighborhood; segmentation; spectral-spatial
classifier
ID REMOTE-SENSING IMAGES; DIRECTIONAL MORPHOLOGICAL PROFILES; SUPPORT
VECTOR MACHINES; MARKOV RANDOM-FIELDS; URBAN AREAS; FEATURE-EXTRACTION;
MATHEMATICAL MORPHOLOGY; CONTEXT CLASSIFICATION; THEORETICAL-ASPECTS;
COMPONENT ANALYSIS
AB Recent advances in spectral-spatial classification of hyperspectral images are presented in this paper. Several techniques are investigated for combining both spatial and spectral information. Spatial information is extracted at the object (set of pixels) level rather than at the conventional pixel level. Mathematical morphology is first used to derive the morphological profile of the image, which includes characteristics about the size, orientation, and contrast of the spatial structures present in the image. Then, the morphological neighborhood is defined and used to derive additional features for classification. Classification is performed with support vector machines (SVMs) using the available spectral information and the extracted spatial information. Spatial postprocessing is next investigated to build more homogeneous and spatially consistent thematic maps. To that end, three presegmentation techniques are applied to define regions that are used to regularize the preliminary pixel-wise thematic map. Finally, a multiple-classifier (MC) system is defined to produce relevant markers that are exploited to segment the hyperspectral image with the minimum spanning forest algorithm. Experimental results conducted on three real hyperspectral images with different spatial and spectral resolutions and corresponding to various contexts are presented. They highlight the importance of spectral-spatial strategies for the accurate classification of hyperspectral images and validate the proposed methods.
C1 [Fauvel, Mathieu] Univ Toulouse, INRA, DYNAFOR Lab, F-31326 Castanet Tolosan, France.
[Tarabalka, Yuliya] INRIA, AYIN, F-06902 Sophia Antipolis, France.
[Benediktsson, Jon Atli] Univ Iceland, Fac Elect & Comp Engn, IS-107 Reykjavik, Iceland.
[Chanussot, Jocelyn] Grenoble Inst Technol, GIPSA Lab, F-38000 Grenoble, France.
[Tilton, James C.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Fauvel, M (reprint author), Univ Toulouse, INRA, DYNAFOR Lab, F-31326 Castanet Tolosan, France.
EM mathieu.fauvel@ensat.fr
RI Benediktsson, Jon/F-2861-2010
OI Benediktsson, Jon/0000-0003-0621-9647
NR 113
TC 294
Z9 310
U1 15
U2 142
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 0018-9219
EI 1558-2256
J9 P IEEE
JI Proc. IEEE
PD MAR
PY 2013
VL 101
IS 3
SI SI
BP 652
EP 675
DI 10.1109/JPROC.2012.2197589
PG 24
WC Engineering, Electrical & Electronic
SC Engineering
GA 097NG
UT WOS:000315480200008
ER
PT J
AU Rojdev, K
O'Rourke, MJE
Hill, C
Nutt, S
Atwell, W
AF Rojdev, Kristina
O'Rourke, Mary Jane E.
Hill, Charles
Nutt, Steven
Atwell, William
TI In-situ strain analysis of potential habitat composites exposed to a
simulated long-term lunar radiation exposure
SO RADIATION PHYSICS AND CHEMISTRY
LA English
DT Article; Proceedings Paper
CT 9th Meeting of the Ionizing Radiation and Polymers (IRaP)
CY OCT 25-29, 2010
CL Univ Maryland, Washington, DC
HO Univ Maryland
DE Composites; Proton; Radiation; Strain; Crosslinking; Scission
ID CHAIN SCISSION; DEGRADATION; POLYMERS; IRRADIATION
AB NASA is studying the effects of long-term space radiation on potential multifunctional composite materials for habitats to better determine their characteristics in harsh space environments. Two epoxy-matrix composite materials were selected for the study and were mounted in a test stand that simulated the biaxial stresses of a pressure vessel wall. The samples in the test stand were exposed to radiation at fast (0.1478 krad/s) and slow (0.0139 krad/s) dose rates, and the strain and temperature were recorded during the exposure. During a fast dose rate exposure, negative strain was recorded, decreasing with time, an indication of matrix shrinkage. Given previous radiation studies of polymers, this is expected to be a result of radiation-induced crosslinking in the epoxy matrix. However, with a slow dose rate, the materials exhibited a positive strain that increased with time, corresponding to stretching of the materials. This result is consistent with scission or degradation of the matrix occurring, possibly due to oxidative degradation. Published by Elsevier Ltd.
C1 [Rojdev, Kristina; O'Rourke, Mary Jane E.; Hill, Charles] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA.
[Rojdev, Kristina; Nutt, Steven] Univ So Calif, Los Angeles, CA 90089 USA.
[Atwell, William] Boeing Co, Houston, TX 77059 USA.
RP Rojdev, K (reprint author), NASA, Lyndon B Johnson Space Ctr, 2101 NASA Pkwy, Houston, TX 77058 USA.
EM kristina.rojdev-1@nasa.gov; MaryJane.E.ORourke@nasa.gov;
charles.s.hill@nasa.gov; nutt@usc.edu; william.atwell@boeing.com
NR 13
TC 0
Z9 0
U1 0
U2 3
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0969-806X
J9 RADIAT PHYS CHEM
JI Radiat. Phys. Chem.
PD MAR
PY 2013
VL 84
BP 235
EP 241
DI 10.1016/j.radphyschem.2012.05.004
PG 7
WC Chemistry, Physical; Nuclear Science & Technology; Physics, Atomic,
Molecular & Chemical
SC Chemistry; Nuclear Science & Technology; Physics
GA 105TJ
UT WOS:000316095100046
ER
PT J
AU Mpagazehe, JN
Street, KW
Delgado, IR
Higgs, CF
AF Mpagazehe, Jeremiah N.
Street, Kenneth W., Jr.
Delgado, Irebert R.
Higgs, C. Fred, III
TI Erosive Wear Characterization of Materia for Lunar Construction
SO TRIBOLOGY & LUBRICATION TECHNOLOGY
LA English
DT Article
C1 [Mpagazehe, Jeremiah N.; Higgs, C. Fred, III] Carnegie Mellon Univ, Dept Mech Engn, Pittsburgh, PA 15213 USA.
[Street, Kenneth W., Jr.; Delgado, Irebert R.] NASA, Glenn Res Ctr, Cleveland, OH USA.
RP Mpagazehe, JN (reprint author), Carnegie Mellon Univ, Dept Mech Engn, Pittsburgh, PA 15213 USA.
EM mpagazehe@cmu.edu
NR 4
TC 0
Z9 0
U1 0
U2 1
PU SOC TRIBOLOGISTS & LUBRICATION ENGINEERS
PI PARK RIDGE
PA 840 BUSSE HIGHWAY, PARK RIDGE, IL 60068 USA
SN 1545-858X
J9 TRIBOL LUBR TECHNOL
JI Tribol. Lubr. Technol.
PD MAR
PY 2013
VL 69
IS 3
BP 19
EP 21
PG 3
WC Engineering, Mechanical
SC Engineering
GA 104GI
UT WOS:000315979500007
ER
PT J
AU Rashki, A
Rautenbach, CJD
Eriksson, PG
Kaskaoutis, DG
Gupta, P
AF Rashki, Alireza
Rautenbach, C. J. deW
Eriksson, Patrik G.
Kaskaoutis, Dimitris G.
Gupta, Pawan
TI Temporal changes of particulate concentration in the ambient air over
the city of Zahedan, Iran
SO AIR QUALITY ATMOSPHERE AND HEALTH
LA English
DT Article
DE Particulate matter; Dust; Mass concentration; Air Quality Index;
Zahedan; Iran
ID NORTH-AFRICAN DUST; SAHARAN DUST; POLLUTION; URBAN; STORM; AEROSOL;
ATHENS; GREECE; CITIES; PM10
AB Air pollution in developing countries has recently become a serious environmental problem, which needs more active air quality monitoring and analyses. To assess air quality characteristics over the city of Zahedan, southeast Iran, airborne particulate matter (PM) concentrations with aerodynamic diameters of < 10, < 2.5, and < 1.0 mu m were measured during the period July 2008 to March 2010 using an Environmental Dust Monitor (EDM-180). The data were analyzed on a daily, monthly, and seasonal basis. The highest monthly mean PM10 levels (172 mu g m(-3)) were recorded during the summer period (June-August), presumably due to frequent dust storms from the nearby Sistan desert located to the north, while less PM10 concentrations are recorded in winter (December-February; 101 mu g m(-3)). Linear regression analysis between the PM2.5 and PM10 time series reveals high correlation coefficients (r > 0.82) for all seasons, implying that PM10 and PM2.5 may have the same source regions or that they are influenced by the same local conditions. In contrast, neutral correlation is found between PM10 and PM1.0 in autumn and winter. Taking into account that the annual variation of PM1.0 exhibits a clear pattern of peaking in winter and dropping in summer (in contrast to PM10), it is suspected that PM1.0 is of different origin than PM10 and mainly influenced by local anthropogenic emissions. The daily PM10 variation is strongly seasonally defined. The maximum PM10 concentrations occur in the morning hours during winter, autumn (September-November), and early spring (March), while in summer, PM10 concentrations increase significantly in the afternoon, closely associated with the intense northerly winds blowing from the desert. As far as the Air Quality Index (AQI) is concerned, its highest monthly values occur in summer, while they are reduced in winter. Desert dust aerosols are found to be the major component in determining the AQI in Zahedan. The analysis shows that 15.3% of the days are unhealthy for sensitive people, while 2% are considered as hazardous.
C1 [Rashki, Alireza; Rautenbach, C. J. deW] Univ Pretoria, Fac Nat & Agr Sci, Dept Geog Geoinformat & Meteorol, ZA-0002 Pretoria, South Africa.
[Eriksson, Patrik G.] Univ Pretoria, Fac Nat & Agr Sci, Dept Geol, ZA-0002 Pretoria, South Africa.
[Kaskaoutis, Dimitris G.] Sharda Univ, Res & Technol Dev Ctr, Greater Noida 201306, India.
[Gupta, Pawan] Univ Maryland Baltimore Cty, Goddard Earth Sci & Technol Ctr, Baltimore, MD 21228 USA.
[Gupta, Pawan] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20770 USA.
RP Rashki, A (reprint author), Univ Pretoria, Fac Nat & Agr Sci, Dept Geog Geoinformat & Meteorol, ZA-0002 Pretoria, South Africa.
EM arrashki@gmail.com
OI Rashki, Alireza/0000-0003-0213-7097
NR 65
TC 12
Z9 12
U1 3
U2 25
PU SPRINGER INTERNATIONAL PUBLISHING AG
PI CHAM
PA GEWERBESTRASSE 11, CHAM, CH-6330, SWITZERLAND
SN 1873-9318
EI 1873-9326
J9 AIR QUAL ATMOS HLTH
JI Air Qual. Atmos. Health
PD MAR
PY 2013
VL 6
IS 1
BP 123
EP 135
DI 10.1007/s11869-011-0152-5
PG 13
WC Environmental Sciences
SC Environmental Sciences & Ecology
GA 095TO
UT WOS:000315357800011
ER
PT J
AU Buckwalter, P
Embaye, T
Gormly, S
Trent, JD
AF Buckwalter, Patrick
Embaye, Tsegereda
Gormly, Sherwin
Trent, Jonathan D.
TI Dewatering microalgae by forward osmosis
SO DESALINATION
LA English
DT Article
DE Osmosis; Microalgae harvesting; Dewatering; Biofouling; Biofuels; OMEGA
ID OSMOTIC CONCENTRATION; MEMBRANE; PERFORMANCE
AB Microalgae are known to be an excellent source of biofuels, but many issues surrounding the scale and economics of their cultivation have yet to be resolved. In particular, dewatering methods, such as centrifugation and tangential flow filtration, are prohibitively energy intensive. In this study, forward osmosis (FO) is considered as a partial dewatering method for microalgae growing on wastewater in a marine environment. Using artificial seawater as the draw solution, average dewatering rates of 2 1/m(2) membrane/h (range 1.8-2.4 1/m(2)h) were observed and volumes decreased by 65-85%. For a single membrane, daily dewatering rates did not significantly change in 14 consecutive experiments. Hourly dewatering rates did not gradually decrease, as might be expected; instead the dewatering rate oscillated throughout each experiment. Exposing an FO membrane in the ocean for 45 days caused significant biofouling on its surface, but its dewatering rate did not change. Exposing three FO membranes in the ocean for 52 days also caused significant biofouling, but in this experiment all membranes developed leaks that allowed saltwater to pass. These experiments suggest that FO may be an energy-saving step in dewatering freshwater microalgae if an appropriate draw solution is available and if conditions are controlled to prevent leakage. Published by Elsevier B.V.
C1 [Buckwalter, Patrick; Gormly, Sherwin] Univ Space Res Assoc, Columbia, MD 21044 USA.
[Embaye, Tsegereda] SETI Inst, Mountain View, CA 94043 USA.
[Trent, Jonathan D.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
RP Trent, JD (reprint author), NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
EM jonathan.d.trent@nasa.gov
FU Google called "Global Research into Energy and the Environment at NASA
(GREEN)"
FX We thank Michael Flynn and Jack Herron for consultation and the staff of
the Capitola Boat and Bait Store for assistance. We thank Brandi McKuin
and Shirley Fauth for editorial assistance. The research was funded
through a collaborative project with Google called "Global Research into
Energy and the Environment at NASA (GREEN)."
NR 19
TC 25
Z9 27
U1 2
U2 85
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0011-9164
J9 DESALINATION
JI Desalination
PD MAR 1
PY 2013
VL 312
SI SI
BP 19
EP 22
DI 10.1016/j.desal.2012.12.015
PG 4
WC Engineering, Chemical; Water Resources
SC Engineering; Water Resources
GA 098KN
UT WOS:000315548300004
ER
PT J
AU Turnbull, M
AF Turnbull, Margaret
TI There is not only one earth. There are many. But we do not know where to
put them all
SO DU
LA German
DT Article
C1 NASA, Washington, DC 20546 USA.
RP Turnbull, M (reprint author), NASA, Washington, DC 20546 USA.
NR 0
TC 0
Z9 0
U1 0
U2 1
PU DU VERLAG
PI SULGEN
PA STEINACKERSTRASSE 8, SULGEN, CH 8583, SWITZERLAND
SN 0012-6837
J9 DU-Z KULTUR
JI Du
PD MAR
PY 2013
IS 834
BP 36
EP 39
PG 4
WC Art
SC Art
GA 098PJ
UT WOS:000315560900003
ER
PT J
AU Stomeo, F
Valverde, A
Pointing, SB
Mckay, CP
Warren-Rhodes, KA
Tuffin, MI
Seely, M
Cowan, DA
AF Stomeo, Francesca
Valverde, Angel
Pointing, Stephen B.
McKay, Christopher P.
Warren-Rhodes, Kimberley A.
Tuffin, Marla I.
Seely, Mary
Cowan, Don A.
TI Hypolithic and soil microbial community assembly along an aridity
gradient in the Namib Desert
SO EXTREMOPHILES
LA English
DT Article
DE Bacteria; Cyanobacteria; Hypoliths; Namib Desert; Niche; Soils
ID MCMURDO DRY VALLEYS; BETA-DIVERSITY; ENVIRONMENTAL GRADIENTS;
COOCCURRENCE PATTERNS; BACTERIAL COMMUNITIES; MULTIVARIATE ANALYSES;
SPECIES COOCCURRENCE; CHINA HOT; ECOLOGY; ANTARCTICA
AB The Namib Desert is considered the oldest desert in the world and hyperarid for the last 5 million years. However, the environmental buffering provided by quartz and other translucent rocks supports extensive hypolithic microbial communities. In this study, open soil and hypolithic microbial communities have been investigated along an East-West transect characterized by an inverse fog-rainfall gradient. Multivariate analysis showed that structurally different microbial communities occur in soil and in hypolithic zones. Using variation partitioning, we found that hypolithic communities exhibited a fog-related distribution as indicated by the significant East-West clustering. Sodium content was also an important environmental factor affecting the composition of both soil and hypolithic microbial communities. Finally, although null models for patterns in microbial communities were not supported by experimental data, the amount of unexplained variation (68-97 %) suggests that stochastic processes also play a role in the assembly of such communities in the Namib Desert.
C1 [Stomeo, Francesca; Valverde, Angel; Tuffin, Marla I.; Cowan, Don A.] Univ Western Cape, IMBM, Cape Town, South Africa.
[Stomeo, Francesca] Int Livestock Res Inst ILRI Hub, BecA, Nairobi 00100, Kenya.
[Valverde, Angel; Cowan, Don A.] Univ Pretoria, Dept Genet, CMEG, ZA-0002 Pretoria, South Africa.
[Pointing, Stephen B.] Auckland Univ Technol, Sch Appl Sci, Auckland 1142, New Zealand.
[McKay, Christopher P.; Warren-Rhodes, Kimberley A.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Seely, Mary] Desert Res Fdn Namibia, Windhoek, Namibia.
RP Cowan, DA (reprint author), Univ Pretoria, Dept Genet, CMEG, ZA-0002 Pretoria, South Africa.
EM f.stomeo@cgiar.org; don.cowan@up.ac.za
RI Valverde, Angel/C-1308-2009; Cowan, Don/E-3991-2012
OI Valverde, Angel/0000-0003-0439-9605; Cowan, Don/0000-0001-8059-861X
FU National Research Foundation (South Africa)
FX The authors gratefully acknowledge F.D. Eckardt for providing Fig. 1a,
and the National Research Foundation (South Africa) for support of this
research.
NR 61
TC 26
Z9 26
U1 4
U2 60
PU SPRINGER JAPAN KK
PI TOKYO
PA CHIYODA FIRST BLDG EAST, 3-8-1 NISHI-KANDA, CHIYODA-KU, TOKYO, 101-0065,
JAPAN
SN 1431-0651
EI 1433-4909
J9 EXTREMOPHILES
JI Extremophiles
PD MAR
PY 2013
VL 17
IS 2
BP 329
EP 337
DI 10.1007/s00792-013-0519-7
PG 9
WC Biochemistry & Molecular Biology; Microbiology
SC Biochemistry & Molecular Biology; Microbiology
GA 098UM
UT WOS:000315574600012
PM 23397517
ER
PT J
AU Babuscia, A
Cheung, KM
AF Babuscia, Alessandra
Cheung, Kar-Ming
TI Statistical Risk Estimation for Communication System Design
SO IEEE SYSTEMS JOURNAL
LA English
DT Article
DE Biases; communication system; density estimation; design risk; expert
elicitation; heuristics; risk analysis
ID PROBABILITY-DISTRIBUTIONS; DENSITY-FUNCTION; UNCERTAINTY
AB Spacecraft is complex systems that involve different subsystems and multiple relationships among them. For these reasons, the design of a spacecraft is an evolutionary process that starts from requirements and evolves over time across different design phases. During this process, a lot of changes can happen. They can affect mass and power at component, subsystem, and system levels. Each spacecraft has to respect the overall constraints in terms of mass and power: for this reason, it is important to be sure that the design does not exceed these limitations. Current practice in the system model primarily deals with this problem by allocating margins on individual components and on individual subsystems. However, a statistical characterization of the fluctuations in mass and power of the overall system (i.e., the spacecraft) is missing. This lack of an adequate statistical characterization would result in a risky spacecraft design that might not fit the mission constraints and requirements, or in a conservative design that might not fully utilize the available resources. Due to the complexity of the problem and due to the different expertise and knowledge required to develop a complete risk model for a spacecraft design, this research is focused on risk estimation for a specific spacecraft subsystem, the communication subsystem. The current research aims to be a "proof of concept" of a risk-based design optimization approach, which can then be further expanded to the design of other subsystems as well as to the whole spacecraft. The objective of this paper is to develop a mathematical approach to quantify the likelihood that the major design drivers of mass and power of a space communication system would meet the spacecraft and mission requirements and constraints through the mission design lifecycle. Using this approach the communication system designers will be able to evaluate and compare different communication architectures in a risk tradeoff prospective. The results described in the presentation include a baseline communication system design tool, and a statistical characterization of the design risks through a combination of historical mission data and expert opinion contributions. An application example of the communication system of a university spacecraft is presented.
C1 [Babuscia, Alessandra] MIT, Space Syst Lab, Cambridge, MA 02139 USA.
[Cheung, Kar-Ming] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Babuscia, A (reprint author), MIT, Space Syst Lab, 77 Massachusetts Ave, Cambridge, MA 02139 USA.
EM babuscia@mit.edu; kar-ming.cheung@jpl.nasa.gov
OI Babuscia, Alessandra/0000-0002-8132-3201
FU Massachusetts Institute of Technology (MIT) Space System Laboratory; MIT
Department of Aeronautics and Astronautics; NASA Jet Propulsion
Laboratory (JPL) through the JPL Graduate Fellowship Program; National
Aeronautics and Space Administration
FX This work was supported in part by the Massachusetts Institute of
Technology (MIT) Space System Laboratory, the MIT Department of
Aeronautics and Astronautics, and the NASA Jet Propulsion Laboratory
(JPL) through the JPL Graduate Fellowship Program. Part of this work was
performed at JPL, California Institute of Technology, Pasadena, under a
contract with the National Aeronautics and Space Administration.
NR 53
TC 2
Z9 2
U1 0
U2 5
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 1932-8184
J9 IEEE SYST J
JI IEEE Syst. J.
PD MAR
PY 2013
VL 7
IS 1
BP 125
EP 136
DI 10.1109/JSYST.2012.2201889
PG 12
WC Computer Science, Information Systems; Engineering, Electrical &
Electronic; Operations Research & Management Science; Telecommunications
SC Computer Science; Engineering; Operations Research & Management Science;
Telecommunications
GA 099SA
UT WOS:000315640400013
ER
PT J
AU Kim, H
Liou, MS
AF Kim, Hyoungjin
Liou, Meng-Sing
TI New fitness sharing approach for multi-objective genetic algorithms
SO JOURNAL OF GLOBAL OPTIMIZATION
LA English
DT Article
DE Genetic algorithms; Multi-objective optimization; Niching; Sharing
Function
ID OPTIMIZATION; SELECTION; SEARCH
AB A novel fitness sharing method for MOGA (Multi-Objective Genetic Algorithm) is proposed by combining a new sharing function and sided degradations in the sharing process, with preference to either of two close solutions. The modified MOGA adopting the new sharing approach is named as MOGAS. Three different variants of MOGAS are tested; MOGASc, MOGASp and MOGASd, favoring children over parents, parents over children and solutions closer to the ideal point, respectively. The variants of MOGAS are compared with MOGA and other state-of-the-art multi-objective evolutionary algorithms such as IBEA, HypE, NSGA-II and SPEA2. The new method shows significant performance improvements from MOGA and is very competitive against other Evolutionary Multi-objective Algorithms (EMOAs) for the ZDT and DTLZ test functions with two and three objectives. Among the three variants MOGASd is found to give the best results for the test problems.
C1 [Kim, Hyoungjin] Sci Applicat Int Corp, Cleveland, OH 44135 USA.
[Liou, Meng-Sing] NASA, Aeroprop Div, Glenn Res Ctr, Cleveland, OH 44135 USA.
RP Kim, H (reprint author), Sci Applicat Int Corp, MS 5-10,21000 Brookpk Rd, Cleveland, OH 44135 USA.
EM hyoungjinkim1@gmail.com
NR 25
TC 4
Z9 10
U1 0
U2 18
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0925-5001
J9 J GLOBAL OPTIM
JI J. Glob. Optim.
PD MAR
PY 2013
VL 55
IS 3
BP 579
EP 595
DI 10.1007/s10898-012-9966-4
PG 17
WC Operations Research & Management Science; Mathematics, Applied
SC Operations Research & Management Science; Mathematics
GA 097XU
UT WOS:000315507600008
ER
PT J
AU Rosenzweig, C
Neofotis, P
AF Rosenzweig, Cynthia
Neofotis, Peter
TI Detection and attribution of anthropogenic climate change impacts
SO WILEY INTERDISCIPLINARY REVIEWS-CLIMATE CHANGE
LA English
DT Review
ID NORTH-ATLANTIC OSCILLATION; LONG-TERM CHANGES; LAND-USE CHANGE;
ATMOSPHERIC CARBON-DIOXIDE; SMALL-MAMMAL COMMUNITIES; NET PRIMARY
PRODUCTION; WESTERN UNITED-STATES; OCEAN ACIDIFICATION; EL-NINO;
PHENOLOGICAL RESPONSE
AB Human-influenced climate change is an observed phenomenon affecting physical and biological systems across the globe. The majority of observed impacts are related to temperature changes and are located in the northern high- and mid-latitudes. However, new evidence is emerging that demonstrates that impacts are related to precipitation changes as well as temperature, and that climate change is impacting systems and sectors beyond the Northern Hemisphere. In this paper, we highlight some of this new evidencefocusing on regions and sectors that the Intergovernmental Panel on Climate Change Fourth Assessment Report (IPCC AR4) noted as under-representedin the context of observed climate change impacts, direct and indirect drivers of change (including carbon dioxide itself), and methods of detection. We also present methods and studies attributing observed impacts to anthropogenic forcing. We argue that the expansion of methods of detection (in terms of a broader array of climate variables and data sources, inclusion of the major modes of climate variability, and incorporation of other drivers of change) is key to discerning the climate sensitivities of sectors and systems in regions where the impacts of climate change currently remain elusive. Attributing such changes to human forcing of the climate system, where possible, is important for development of effective mitigation and adaptation. Current challenges in documenting adaptation and the role of indigenous knowledge in detection and attribution are described. (C) 2013 John Wiley & Sons, Ltd. WIREs Clim Change 2013, 4:121150. doi: 10.1002/wcc.209 For further resources related to this article, please visit the WIREs website.
C1 [Rosenzweig, Cynthia] NASA, Goddard Inst Space Studies, Climate Impacts Grp, New York, NY 10025 USA.
[Neofotis, Peter] CUNY Brooklyn Coll, Dept Biol Sci, Brooklyn, NY 11210 USA.
[Neofotis, Peter] CUNY Grad Sch & Univ Ctr, New York, NY 10036 USA.
RP Rosenzweig, C (reprint author), NASA, Goddard Inst Space Studies, Climate Impacts Grp, New York, NY 10025 USA.
EM cynthia.rosenzweig@nasa.gov
FU NASA Earth Science Division through the office of Dr. Jack A. Kaye
FX We gratefully acknowledge Dr. Marta Vicarelli for spatial analysis,
Soyee Chiu for research assistance, Tommy J Moorman for scientific
illustration, and Jose Mendoza for graphics. We thank the editors,
especially Dr. Timothy R. Carter, and anonymous reviewers for their
astute comments and suggestions on this manuscript. Support was provided
by the NASA Earth Science Division through the office of Dr. Jack A.
Kaye.
NR 206
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U2 161
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 1757-7780
EI 1757-7799
J9 WIRES CLIM CHANGE
JI Wiley Interdiscip. Rev.-Clim. Chang.
PD MAR-APR
PY 2013
VL 4
IS 2
BP 121
EP 150
DI 10.1002/wcc.209
PG 30
WC Environmental Studies; Meteorology & Atmospheric Sciences
SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences
GA 097IF
UT WOS:000315466500005
ER
PT J
AU Parker, JS
Anderson, RL
AF Parker, Jeffrey S.
Anderson, Rodney L.
TI Targeting low-energy transfers to low lunar orbit
SO ACTA ASTRONAUTICA
LA English
DT Article
DE Earth Moon; Low-energy transfers; Lunar transfers; Low lunar orbit;
Mission design; Dynamical systems; Three-body trajectories
ID MOON; TRAJECTORIES; CAPTURE; MISSION
AB A targeting scheme is presented to build 21-day launch periods for low-energy trajectories from any specified Earth parking orbit to any specified low lunar orbit, using up to two mid-course maneuvers. A total of 288 launch periods are constructed for transfers to a variety of different targeted low lunar orbits, arriving at different times during the month. Each orbital insertion occurs at an altitude of 100 km above the lunar surface and each orbit sampled in this paper is polar; the longitude of ascending node and the argument of periapse vary for each sampled orbit. An analysis is presented to characterize the total transfer Delta V required to build a launch period, as well as the total transfer Delta V required to transfer from any given Earth parking orbit inclination to each sampled lunar orbit. (C) 2012 Published by Elsevier Ltd. on behalf of IAA.
C1 [Parker, Jeffrey S.; Anderson, Rodney L.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Parker, JS (reprint author), 1860 Athens St,Apt 1, Boulder, CO 80302 USA.
EM parkerjs@gmail.com; Rodney.L.Anderson@jpl.nasa.gov
OI Anderson, Rodney/0000-0001-5336-2775
FU National Aeronautics and Space Administration
FX The research presented in this paper has been carried out at the Jet
Propulsion Laboratory, California Institute of Technology, under a
contract with the National Aeronautics and Space Administration.
Government sponsorship acknowledged.
NR 39
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PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0094-5765
J9 ACTA ASTRONAUT
JI Acta Astronaut.
PD MAR-APR
PY 2013
VL 84
BP 1
EP 14
DI 10.1016/j.actaastro.2012.10.033
PG 14
WC Engineering, Aerospace
SC Engineering
GA 091VL
UT WOS:000315077800001
ER
PT J
AU Landis, RR
Abell, PA
Adamo, DR
Barbee, BW
Johnson, LN
AF Landis, Rob R.
Abell, Paul A.
Adamo, Daniel R.
Barbee, Brent W.
Johnson, Lindley N.
TI The first steps towards a de minimus, affordable NEA exploration
architecture
SO ACTA ASTRONAUTICA
LA English
DT Article
DE Asteroids; Exploration; NEOs; Survey; Spacecraft; Astronauts
ID EARTH OBJECTS; HAYABUSA; ITOKAWA; SPACECRAFT
AB The impetus for asteroid exploration is scientific, political, and pragmatic. The notion of sending human explorers to asteroids is not new. Piloted missions to these primitive bodies were first discussed in the 1960s, pairing Saturn V rockets with enhanced Apollo spacecraft to explore what were then called "Earth-approaching asteroids." Two decades ago, NASA's Space Exploration Initiative (SEI) also briefly examined the possibility of visiting these small celestial bodies. Most recently, the US Human Space Flight Review Committee (the second Augustine Commission) suggested that near-Earth objects (NEOs) represent a target-rich environment for exploration via the "Flexible Path" option. However, prior to seriously considering human missions to NEOs, it has become clear that we currently lack a robust catalog of human-accessible targets. The majority of the known NEOs identified by a study team across several NASA centers as "human-accessible" are probably too small and have orbits that are too uncertain to consider mounting piloted expeditions to these small worlds. The first step in developing a comprehensive catalog is, therefore, to complete a space-based NEO survey. The resulting catalog of candidate NEOs would then be transformed into a matrix of opportunities for robotic and human missions for the next several decades and shared with the international community. This initial step of a space-based NEO survey is therefore the linchpin to laying the foundation of a low-risk architecture to venture out and explore these primitive bodies. We suggest such a minimalist framework architecture from (1) extensive ground-based and precursor spacecraft investigations (while applying operational knowledge from science-driven robotic missions), (2) astronaut servicing of spacecraft operating at geosynchronous Earth orbit to retain essential skills and experience, and (3) applying the sum of these skills, knowledge and experience to piloted missions to NEOs. Published by Elsevier Ltd. on behalf of IAA.
C1 [Landis, Rob R.] NASA, Goddard Space Flight Ctr, Wallops Flight Facil, Wallops Isl, VA 23337 USA.
[Abell, Paul A.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA.
[Adamo, Daniel R.] Trajectory Consultant, Houston, TX USA.
[Barbee, Brent W.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Johnson, Lindley N.] NASA Headquarters, Washington, DC USA.
RP Landis, RR (reprint author), NASA, Goddard Space Flight Ctr, Wallops Flight Facil, Wallops Isl, VA 23337 USA.
EM rob.r.landis@nasa.gov
NR 35
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PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0094-5765
J9 ACTA ASTRONAUT
JI Acta Astronaut.
PD MAR-APR
PY 2013
VL 84
BP 161
EP 172
DI 10.1016/j.actaastro.2012.10.006
PG 12
WC Engineering, Aerospace
SC Engineering
GA 091VL
UT WOS:000315077800016
ER
PT J
AU Youngquist, RC
Nurge, MA
Starr, SO
AF Youngquist, Robert C.
Nurge, Mark A.
Starr, Stanley O.
TI Alternating magnetic field forces for satellite formation flying
SO ACTA ASTRONAUTICA
LA English
DT Article
DE Spacecraft formation flying; Satellite propulsion; Antenna forces;
Electromagnetic forces; Satellite positioning; Space telescopes
ID COILS
AB Selected future space missions, such as large aperture telescopes and multi-component interferometers, will require the precise positioning of a number of isolated satellites, yet many of the suggested approaches for providing satellite positioning forces have serious limitations. In this paper we propose a new approach, capable of providing both position and orientation forces, that resolves or alleviates many of these problems. We show that by using alternating fields and currents that finely-controlled forces can be induced on the satellites, which can be individually selected through frequency allocation. We also show, through analysis and experiment, that near field operation is feasible and can provide sufficient force and the necessary degrees of freedom to accurately position and orient small satellites relative to one another. In particular, the case of a telescope with a large number of free mirrors is developed to provide an example of the concept. We also discuss the far field extension of this concept. Published by Elsevier Ltd. on behalf of IAA.
C1 [Youngquist, Robert C.; Nurge, Mark A.; Starr, Stanley O.] NASA, Kennedy Space Ctr, FL 32899 USA.
RP Nurge, MA (reprint author), NASA, Mail Stop NE L5, Kennedy Space Ctr, FL 32899 USA.
EM Mark.A.Nurge@nasa.gov
FU NASA Office of the Chief Technologist
FX We wish to thank Rick Birr for RF support and Robert Cox and Mike Csonka
for aid in constructing test equipment. This work was supported by the
NASA Office of the Chief Technologist.
NR 15
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PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0094-5765
J9 ACTA ASTRONAUT
JI Acta Astronaut.
PD MAR-APR
PY 2013
VL 84
BP 197
EP 205
DI 10.1016/j.actaastro.2012.11.012
PG 9
WC Engineering, Aerospace
SC Engineering
GA 091VL
UT WOS:000315077800020
ER
PT J
AU Brown, ME
Silver, KC
Rajagopalan, K
AF Brown, Molly E.
Silver, Kirk C.
Rajagopalan, Krishnan
TI A city and national metric measuring isolation from the global market
for food security assessment
SO APPLIED GEOGRAPHY
LA English
DT Article
DE Transportation; Food security; Global market; Index; Economics
ID AGRICULTURE; POVERTY
AB The World Bank has invested in infrastructure in developing countries for decades. This investment aims to reduce the isolation of markets, reducing both seasonality and variability in food availability and food prices. Here we combine city market price data, global distance to port, and country infrastructure data to create a new Isolation Index for countries and cities around the world. Our index quantifies the isolation of a city from the global market. We demonstrate that an index built at the country level can be applied at a sub-national level to quantify city isolation. In doing so, we offer policy makers with an alternative metric to assess food insecurity. We compare our isolation index with other indices and economic data found in the literature. We show that our Index measures economic isolation regardless of economic stability using correlation and analysis. Published by Elsevier Ltd.
C1 [Brown, Molly E.] NASA, Goddard Space Flight Ctr, Biospher Sci Lab, Greenbelt, MD 20771 USA.
[Silver, Kirk C.] Univ Rhode Isl, Coll Environm & Life Sci, Coastal Inst MESM 106, Kingston, RI 02881 USA.
[Rajagopalan, Krishnan] USN Acad, Dept Math, Annapolis, MD 21402 USA.
RP Brown, ME (reprint author), NASA, Goddard Space Flight Ctr, Biospher Sci Lab, Code 618, Greenbelt, MD 20771 USA.
EM molly.brown@nasa.gov
RI Brown, Molly/E-2724-2010
OI Brown, Molly/0000-0001-7384-3314
NR 34
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PU ELSEVIER SCI LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND
SN 0143-6228
J9 APPL GEOGR
JI Appl. Geogr.
PD MAR
PY 2013
VL 38
BP 119
EP 128
DI 10.1016/j.apgeog.2012.11.015
PG 10
WC Geography
SC Geography
GA 094FI
UT WOS:000315248000012
ER
PT J
AU Wright, EL
Skrutskie, MF
Kirkpatrick, JD
Gelino, CR
Griffith, RL
Marsh, KA
Jarrett, T
Nelson, MJ
Borish, HJ
Mace, G
Mainzer, AK
Eisenhardt, PR
McLean, IS
Tobin, JJ
Cushing, MC
AF Wright, Edward L.
Skrutskie, M. F.
Kirkpatrick, J. Davy
Gelino, Christopher R.
Griffith, Roger L.
Marsh, Kenneth A.
Jarrett, Tom
Nelson, M. J.
Borish, H. J.
Mace, Gregory
Mainzer, Amanda K.
Eisenhardt, Peter R.
McLean, Ian S.
Tobin, John J.
Cushing, Michael C.
TI A T8.5 BROWN DWARF MEMBER OF THE xi URSAE MAJORIS SYSTEM
SO ASTRONOMICAL JOURNAL
LA English
DT Article
DE brown dwarfs; infrared: stars; solar neighborhood; stars: late-type;
stars: low-mass
ID SPITZER-SPACE-TELESCOPE; ADAPTIVE OPTICS SYSTEM; INFRARED ARRAY CAMERA;
SURVEY-EXPLORER WISE; T-DWARFS; SPECTRAL CLASSIFICATION; DYNAMICAL
MASSES; PROPER MOTIONS; BINARY ORBITS; STARS
AB The Wide-field Infrared Survey Explorer has revealed a T8.5 brown dwarf (WISE J111838.70+312537.9) that exhibits common proper motion with a solar-neighborhood (8 pc) quadruple star system-xi Ursae Majoris. The angular separation is 8'.5, and the projected physical separation is approximate to 4000 AU. The sub-solar metallicity and low chromospheric activity of xi UMa A argue that the system has an age of at least 2 Gyr. The infrared luminosity and color of the brown dwarf suggests the mass of this companion ranges between 14 and 38 M-J for system ages of 2 and 8 Gyr, respectively.
C1 [Wright, Edward L.; Mace, Gregory; McLean, Ian S.] UCLA Astron, Los Angeles, CA 90095 USA.
[Skrutskie, M. F.; Nelson, M. J.; Borish, H. J.] Univ Virginia, Dept Astron, Charlottesville, VA 22904 USA.
[Kirkpatrick, J. Davy; Gelino, Christopher R.; Griffith, Roger L.; Jarrett, Tom] CALTECH, Ctr Infrared Proc & Anal, Pasadena, CA 91125 USA.
[Marsh, Kenneth A.] Cardiff Univ, Sch Phys & Astron, Cardiff CF2 43AA, S Glam, Wales.
[Mainzer, Amanda K.; Eisenhardt, Peter R.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Tobin, John J.] Natl Radio Astron Observ, Charlottesville, VA 22903 USA.
[Cushing, Michael C.] Univ Toledo, Dept Phys & Astron, Toledo, OH 43606 USA.
RP Wright, EL (reprint author), UCLA Astron, POB 951547, Los Angeles, CA 90095 USA.
EM wright@astro.ucla.edu
FU National Aeronautics and Space Administration; NASA Keck PI Data Award;
W. M. Keck Foundation
FX This publication makes use of data products from the Widefield Infrared
Survey Explorer, which is a joint project of the University of
California, Los Angeles, and the Jet Propulsion Laboratory/California
Institute of Technology, funded by the National Aeronautics and Space
Administration.; This work was partially supported by a NASA Keck PI
Data Award, administered by the NASA Exoplanet Science Institute. Part
of the data presented herein were obtained at the W. M. Keck Observatory
from telescope time allocated to the National Aeronautics and Space
Administration through the agency's scientific partnership with the
California Institute of Technology and the University of California. The
Observatory was made possible by the generous financial support of the
W. M. Keck Foundation. The authors wish to recognize and acknowledge the
very significant cultural role and reverence that the summit of Mauna
Kea has always had within the indigenous Hawaiian community. We are most
fortunate to have the opportunity to conduct observations from this
mountain.
NR 48
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PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-6256
J9 ASTRON J
JI Astron. J.
PD MAR
PY 2013
VL 145
IS 3
AR 84
DI 10.1088/0004-6256/145/3/84
PG 8
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 089XU
UT WOS:000314944100032
ER
PT J
AU Yan, L
Donoso, E
Tsai, CW
Stern, D
Assef, RJ
Eisenhardt, P
Blain, AW
Cutri, R
Jarrett, T
Stanford, SA
Wright, E
Bridge, C
Riechers, DA
AF Yan, Lin
Donoso, E.
Tsai, Chao-Wei
Stern, D.
Assef, R. J.
Eisenhardt, P.
Blain, A. W.
Cutri, R.
Jarrett, T.
Stanford, S. A.
Wright, E.
Bridge, C.
Riechers, D. A.
TI CHARACTERIZING THE MID-INFRARED EXTRAGALACTIC SKY WITH WISE AND SDSS
SO ASTRONOMICAL JOURNAL
LA English
DT Article
DE galaxies: evolution; galaxies: high-redshift; galaxies: starburst;
infrared: galaxies
ID ACTIVE GALACTIC NUCLEI; SPECTROSCOPIC TARGET SELECTION; IRAC SHALLOW
SURVEY; 7TH DATA RELEASE; X-RAY; LUMINOSITY FUNCTION; DEEP SURVEY; MU-M;
GALAXIES; REDSHIFT
AB The Wide-field Infrared Survey Explorer (WISE) has completed its all-sky survey in four channels at 3.4-22 mu m, detecting hundreds of millions of objects. We merge the WISE mid-infrared data with optical data from the Sloan Digital Sky Survey (SDSS) and provide a phenomenological characterization of WISE extragalactic sources. WISE is most sensitive at 3.4 mu m (W1) and least sensitive at 22 mu m (W4). The W1 band probes massive early-type galaxies out to z greater than or similar to 1. This is more distant than SDSS identified early-type galaxies, consistent with the fact that 28% of 3.4 mu m sources have faint or no r-band counterparts (r > 22.2). In contrast, 92%-95% of 12 mu m and 22 mu m sources have SDSS optical counterparts with r <= 22.2. WISE 3.4 mu m detects 89.8% of the entire SDSS QSO catalog at S/N-W1 > 7 sigma, but only 18.9% at 22 mu m with S/N-W4 > 5 sigma. We show that WISE colors alone are effective in isolating stars (or local early-type galaxies), star-forming galaxies, and strong active galactic nuclei (AGNs)/QSOs at z less than or similar to 3. We highlight three major applications of WISE colors: (1) Selection of strong AGNs/QSOs at z <= 3 using W1- W2 > 0.8 and W2 < 15.2 criteria, producing a better census of this population. The surface density of these strong AGN/QSO candidates is 67.5 +/- 0.14 deg(-2). (2) Selection of dust-obscured, type-2 AGN/QSO candidates. We show that WISE W1 - W2 > 0.8, W2 < 15.2 combined with r - W2 > 6 (Vega) colors can be used to identify type-2 AGN candidates. The fraction of these type-2 AGN candidates is one-third of all WISE color-selected AGNs. (3) Selection of ultraluminous infrared galaxies (ULIRGs) at z similar to 2 with extremely red colors, r - W4 > 14 or well-detected 22 mu m sources lacking detections in the 3.4 and 4.6 mu m bands. The surface density of z similar to 2 ULIRG candidates selected with r - W4 > 14 is 0.9 +/- 0.07 deg(-2) at S/N-W4 >= 5 (the corresponding, lowest flux density of 2.5 mJy), which is consistent with that inferred from smaller area Spitzer surveys. Optical spectroscopy of a small number of these high-redshift ULIRG candidates confirms our selection, and reveals a possible trend that optically fainter or r - W4 redder candidates are at higher redshifts.
C1 [Yan, Lin; Donoso, E.; Tsai, Chao-Wei; Cutri, R.; Jarrett, T.] CALTECH, Infrared Proc & Anal Ctr, Pasadena, CA 91125 USA.
[Stern, D.; Assef, R. J.; Eisenhardt, P.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Blain, A. W.] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England.
[Stanford, S. A.] Univ Calif Davis, Dept Phys, Davis, CA 95616 USA.
[Wright, E.] Univ Calif Los Angeles, Dept Astron, Los Angeles, CA 90095 USA.
[Bridge, C.; Riechers, D. A.] CALTECH, Dept Astron, Pasadena, CA 91125 USA.
[Riechers, D. A.] Cornell Univ, Dept Astron, Ithaca, NY 14853 USA.
RP Yan, L (reprint author), CALTECH, Infrared Proc & Anal Ctr, MS 100-22, Pasadena, CA 91125 USA.
EM lyan@ipac.caltech.edu
NR 62
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PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-6256
J9 ASTRON J
JI Astron. J.
PD MAR
PY 2013
VL 145
IS 3
AR 55
DI 10.1088/0004-6256/145/3/55
PG 16
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 089XU
UT WOS:000314944100003
ER
PT J
AU Loomis, RA
Zaleski, DP
Steber, AL
Neill, JL
Muckle, MT
Harris, BJ
Hollis, JM
Jewell, PR
Lattanzi, V
Lovas, FJ
Martinez, O
McCarthy, MC
Remijan, AJ
Pate, BH
Corby, JF
AF Loomis, Ryan A.
Zaleski, Daniel P.
Steber, Amanda L.
Neill, Justin L.
Muckle, Matthew T.
Harris, Brent J.
Hollis, Jan M.
Jewell, Philip R.
Lattanzi, Valerio
Lovas, Frank J.
Martinez, Oscar, Jr.
McCarthy, Michael C.
Remijan, Anthony J.
Pate, Brooks H.
Corby, Joanna F.
TI THE DETECTION OF INTERSTELLAR ETHANIMINE (CH3CHNH) FROM OBSERVATIONS
TAKEN DURING THE GBT PRIMOS SURVEY
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE catalogs; ISM: abundances; ISM: individual objects (SgrB2N); ISM:
molecules; methods: laboratory; surveys
ID TRANSFORM MICROWAVE SPECTROMETER; ICE ANALOGS; CHIRPED-PULSE;
AMINO-ACIDS; HYDROGEN-CYANIDE; SAGITTARIUS B2; LINE SURVEY; GAS-PHASE;
ORION-KL; SPECTRUM
AB We have performed reaction product screening measurements using broadband rotational spectroscopy to identify rotational transition matches between laboratory spectra and the Green Bank Telescope PRIMOS radio astronomy survey spectra in Sagittarius B2 North (Sgr B2(N)). The broadband rotational spectrum of molecules created in an electrical discharge of CH3CN and H2S contained several frequency matches to unidentified features in the PRIMOS survey that did not have molecular assignments based on standard radio astronomy spectral catalogs. Several of these transitions are assigned to the E- and Z-isomers of ethanimine. Global fits of the rotational spectra of these isomers in the range of 8-130 GHz have been performed for both isomers using previously published mm-wave spectroscopy measurements and the microwave measurements of the current study. Possible interstellar chemistry formation routes for E- ethanimine and Z- ethanimine are discussed. The detection of ethanimine is significant because of its possible role in the formation of alanine-one of the twenty amino acids in the genetic code.
C1 [Loomis, Ryan A.; Zaleski, Daniel P.; Steber, Amanda L.; Neill, Justin L.; Muckle, Matthew T.; Harris, Brent J.; Pate, Brooks H.] Univ Virginia, Dept Chem, Charlottesville, VA 22904 USA.
[Hollis, Jan M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Jewell, Philip R.; Remijan, Anthony J.] Natl Radio Astron Observ, Charlottesville, VA 22904 USA.
[Lattanzi, Valerio; Martinez, Oscar, Jr.; McCarthy, Michael C.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Lattanzi, Valerio; Martinez, Oscar, Jr.; McCarthy, Michael C.] Harvard Univ, Sch Engn & Appl Sci, Cambridge, MA 02138 USA.
[Lovas, Frank J.] NIST, Gaithersburg, MD 20899 USA.
[Corby, Joanna F.] Univ Virginia, Dept Astron, Charlottesville, VA 22904 USA.
RP Loomis, RA (reprint author), Univ Virginia, Dept Chem, McCormick Rd, Charlottesville, VA 22904 USA.
OI McCarthy, Michael/0000-0001-9142-0008; Steber,
Amanda/0000-0002-8203-2174; Zaleski, Daniel/0000-0003-0153-9158
FU Centers for Chemical Innovation program of the National Science
Foundation [CHE-0847919]; NSF Chemistry [CHE-1213200]; College Science
Scholars program at the University of Virginia
FX The authors acknowledge support from the Centers for Chemical Innovation
program of the National Science Foundation (CHE-0847919), NSF Chemistry
(CHE-1213200), and the College Science Scholars program at the
University of Virginia. We also thank B. McGuire and R. Pulliam for
helpful comments to improve the manuscript. Finally, we thank the
anonymous referee for valuable comments and suggestions on the
manuscript. The National Radio Astronomy Observatory is a facility of
the National Science Foundation operated under cooperative agreement by
Associated Universities, Inc.
NR 43
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PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 2041-8205
J9 ASTROPHYS J LETT
JI Astrophys. J. Lett.
PD MAR 1
PY 2013
VL 765
IS 1
AR L9
DI 10.1088/2041-8205/765/1/L9
PG 7
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 093JK
UT WOS:000315187800009
ER
PT J
AU Zaleski, DP
Seifert, NA
Steber, AL
Muckle, MT
Loomis, RA
Corby, JF
Martinez, O
Crabtree, KN
Jewell, PR
Hollis, JM
Lovas, FJ
Vasquez, D
Nyiramahirwe, J
Sciortino, N
Johnson, K
McCarthy, MC
Remijan, AJ
Pate, BH
AF Zaleski, Daniel P.
Seifert, Nathan A.
Steber, Amanda L.
Muckle, Matt T.
Loomis, Ryan A.
Corby, Joanna F.
Martinez, Oscar, Jr.
Crabtree, Kyle N.
Jewell, Philip R.
Hollis, Jan M.
Lovas, Frank J.
Vasquez, David
Nyiramahirwe, Jolie
Sciortino, Nicole
Johnson, Kennedy
McCarthy, Michael C.
Remijan, Anthony J.
Pate, Brooks H.
TI DETECTION OF E-CYANOMETHANIMINE TOWARD SAGITTARIUS B2(N) IN THE GREEN
BANK TELESCOPE PRIMOS SURVEY
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE catalogs; ISM: abundances; ISM: individual objects (SgrB2N); ISM:
molecules; methods: laboratory; surveys
ID SPECTRAL-LINE SURVEY; Z-C-CYANOMETHANIMINE; OBSERVATIONAL DATA;
ORGANIC-MOLECULES; MICROWAVE-SPECTRA; PRIMITIVE EARTH; HCN DIMER;
INTERSTELLAR; DELIVERY; ADENINE
AB The detection of E-cyanomethanimine (E-HNCHCN) toward Sagittarius B2(N) is made by comparing the publicly available Green Bank Telescope (GBT) PRIMOS survey spectra to laboratory rotational spectra from a reaction product screening experiment. The experiment uses broadband molecular rotational spectroscopy to monitor the reaction products produced in an electric discharge source using a gas mixture of NH3 and CH3CN. Several transition frequency coincidences between the reaction product screening spectra and previously unassigned interstellar rotational transitions in the PRIMOS survey have been assigned to E-cyanomethanimine. A total of eight molecular rotational transitions of this molecule between 9 and 50 GHz are observed with the GBT. E-cyanomethanimine, often called the HCN dimer, is an important molecule in prebiotic chemistry because it is a chemical intermediate in proposed synthetic routes of adenine, one of the two purine nucleobases found in DNA and RNA. New analyses of the rotational spectra of both E-cyanomethanimine and Z-cyanomethanimine that incorporate previous millimeter-wave measurements are also reported.
C1 [Zaleski, Daniel P.; Seifert, Nathan A.; Steber, Amanda L.; Muckle, Matt T.; Loomis, Ryan A.; Vasquez, David; Nyiramahirwe, Jolie; Sciortino, Nicole; Johnson, Kennedy; Pate, Brooks H.] Univ Virginia, Dept Chem, Charlottesville, VA 22904 USA.
[Corby, Joanna F.] Univ Virginia, Dept Astron, Charlottesville, VA 22904 USA.
[Martinez, Oscar, Jr.; Crabtree, Kyle N.; McCarthy, Michael C.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Martinez, Oscar, Jr.; Crabtree, Kyle N.; McCarthy, Michael C.] Harvard Univ, Sch Engn & Appl Sci, Cambridge, MA 02138 USA.
[Jewell, Philip R.; Remijan, Anthony J.] Natl Radio Astron Observ, Charlottesville, VA 22903 USA.
[Hollis, Jan M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Lovas, Frank J.] NIST, Gaithersburg, MD 20899 USA.
RP Zaleski, DP (reprint author), Univ Virginia, Dept Chem, McCormick Rd, Charlottesville, VA 22904 USA.
EM bp2k@virginia.edu; mccarthy@cfa.harvard.edu; aremijan@nrao.edu
OI Crabtree, Kyle/0000-0001-5629-5192; McCarthy,
Michael/0000-0001-9142-0008; Steber, Amanda/0000-0002-8203-2174;
Zaleski, Daniel/0000-0003-0153-9158
FU NSF Centers for Chemical Innovation [CHE-0847919]; NSF Chemistry
[CHE-1213200]; Virginia-North Carolina Alliance, a NSF Louis Stokes
Alliance for Minority Participation [HRD-1202181]; National Radio
Astronomy Observatory
FX This work was supported by the NSF Centers for Chemical Innovation
(CHE-0847919) and NSF Chemistry (CHE-1213200). Additional support was
provided by the Virginia-North Carolina Alliance, a NSF Louis Stokes
Alliance for Minority Participation (HRD-1202181) and the National Radio
Astronomy Observatory. The National Radio Astronomy Observatory is a
facility of the National Science Foundation operated under cooperative
agreement by Associated Universities, Inc. Finally, we thank the
anonymous referee for a favorable review and valuable comments that
greatly improved the quality of this manuscript.
NR 36
TC 26
Z9 26
U1 1
U2 22
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 2041-8205
J9 ASTROPHYS J LETT
JI Astrophys. J. Lett.
PD MAR 1
PY 2013
VL 765
IS 1
AR L10
DI 10.1088/2041-8205/765/1/L10
PG 6
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 093JK
UT WOS:000315187800010
ER
PT J
AU Wang, LH
Newchurch, MJ
Pour-Biazar, A
Kuang, S
Khan, M
Liu, X
Koshak, W
Chance, K
AF Wang, Lihua
Newchurch, M. J.
Pour-Biazar, Arastoo
Kuang, Shi
Khan, Maudood
Liu, Xiong
Koshak, William
Chance, Kelly
TI Estimating the influence of lightning on upper tropospheric ozone using
NLDN lightning data and CMAQ model
SO ATMOSPHERIC ENVIRONMENT
LA English
DT Article
DE LNOx; CMAQ; Ozone; Lightning; NLDN; OMI; IONS06
ID CONTINENTAL UNITED-STATES; NITROGEN-OXIDES; NOX PRODUCTION; MONITORING
INSTRUMENT; PROFILE RETRIEVALS; GENERATED NOX; STERAO-A; TRANSPORT;
THUNDERSTORMS; MIDLATITUDES
AB Lightning is a particularly significant NOx source in the middle and upper troposphere where it affects tropospheric chemistry and ozone. Because the version-4 Community Multiscale Air Quality Modeling System (CMAQ) does not account for NOx emission from lightning, it underpredicts NOx above the mixed layer. In this study, the National Lightning Detection Network (TM) (NLDN) lightning data are applied to the CMAQ model to simulate the influence of lightning-produced NOx (LNOx) on upper tropospheric NOx and subsequent ozone concentration. Using reasonable values for salient parameters (detection efficiency similar to 95%, cloud flash to ground flash ratio similar to 3, LNOx production rate similar to 500 mol N per flash), the NLDN ground flashes are converted into total lightning NOx amount and then vertically distributed on 39 CMAQ model layers according to a vertical-distribution profile of lightning N mass. This LNOx contributes 27% of the total NOx emission during 15 July similar to 7 September 2006. This additional NOx reduces the low-bias of simulated tropospheric O-3 columns with respect to OMI tropospheric O-3 columns from 10 to 5%. Although the model prediction of ozone in upper troposphere improves by similar to 20 ppbv due to lightning-produced NOx above the southeastern and eastern U.S.A., the improved ozone prediction is still similar to 20-25 ppbv lower than ozonesonde measurements. (C) 2012 Elsevier Ltd. All rights reserved.
C1 [Wang, Lihua; Newchurch, M. J.; Pour-Biazar, Arastoo; Kuang, Shi] Univ Alabama, Huntsville, AL 35899 USA.
[Khan, Maudood] NASA, George C Marshall Space Flight Ctr, Univ Space Res Assoc, Huntsville, AL 35812 USA.
[Liu, Xiong; Chance, Kelly] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Koshak, William] NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA.
RP Wang, LH (reprint author), Univ Alabama, Huntsville, AL 35899 USA.
EM lihuawang@nsstc.uah.edu
RI Liu, Xiong/P-7186-2014;
OI Liu, Xiong/0000-0003-2939-574X; Chance, Kelly/0000-0002-7339-7577
FU Minerals Management Service; Minerals Management Service on Gulf of
Mexico Issues; NASA Science Mission Directorate Applied Sciences
Program; Atmospheric Chemistry Program; NOAA/NESDIS
FX This work is supported by the Minerals Management Service under
Cooperative Agreement between the University of Alabama in Huntsville
and the Minerals Management Service on Gulf of Mexico Issues, the NASA
Science Mission Directorate Applied Sciences Program and Atmospheric
Chemistry Program, and NOAA/NESDIS.
NR 63
TC 5
Z9 5
U1 1
U2 33
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 1352-2310
J9 ATMOS ENVIRON
JI Atmos. Environ.
PD MAR
PY 2013
VL 67
BP 219
EP 228
DI 10.1016/j.atmosenv.2012.11.001
PG 10
WC Environmental Sciences; Meteorology & Atmospheric Sciences
SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences
GA 093EA
UT WOS:000315173300026
ER
PT J
AU Oltmans, SJ
Lefohn, AS
Shadwick, D
Harris, JM
Scheel, HE
Galbally, I
Tarasick, DW
Johnson, BJ
Brunke, EG
Claude, H
Zeng, G
Nichol, S
Schmidlin, F
Davies, J
Cuevas, E
Redondas, A
Naoe, H
Nakano, T
Kawasato, T
AF Oltmans, S. J.
Lefohn, A. S.
Shadwick, D.
Harris, J. M.
Scheel, H. E.
Galbally, I.
Tarasick, D. W.
Johnson, B. J.
Brunke, E. -G.
Claude, H.
Zeng, G.
Nichol, S.
Schmidlin, F.
Davies, J.
Cuevas, E.
Redondas, A.
Naoe, H.
Nakano, T.
Kawasato, T.
TI Recent tropospheric ozone changes - A pattern dominated by slow or no
growth
SO ATMOSPHERIC ENVIRONMENT
LA English
DT Article
DE Troposphere ozone; Trends; Changes in concentration distribution
ID LONG-TERM CHANGES; UNITED-STATES; SURFACE OZONE; NORTH-AMERICA;
BACKGROUND OZONE; INCREASING OZONE; RURAL SITES; WEST-COAST; TRENDS;
REDUCTION
AB Longer-term (i.e., 20-40 years) tropospheric ozone (O-3) time series obtained from surface and ozonesonde observations have been analyzed to assess possible changes with time through 2010. The time series have been selected to reflect relatively broad geographic regions and where possible minimize local scale influences, generally avoiding sites close to larger urban areas. Several approaches have been used to describe the changes with time, including application of a time series model, running 15-year trends, and changes in the distribution by month in the O-3 mixing ratio. Changes have been investigated utilizing monthly averages, as well as exposure metrics that focus on specific parts of the distribution of hourly average concentrations (e.g., low-, mid-, and high-level concentration ranges). Many of the longer time series (similar to 30 years) in mid-latitudes of the Northern Hemisphere, including those in Japan, show a pattern of significant increase in the earlier portion of the record, with a flattening over the last 10-15 years. It is uncertain if the flattening of the O-3 change over Japan reflects the impact of O-3 transported from continental East Asia in light of reported O-3 increases in China. In the Canadian Arctic, declines from the beginning of the ozonesonde record in 1980 have mostly rebounded with little overall change over the period of record. The limited data in the tropical Pacific suggest very little change over the entire record. In the southern hemisphere subtropics and mid-latitudes, the significant increase observed in the early part of the record has leveled off in the most recent decade. At the South Pole, a decline observed during the first half of the 35-year record has reversed, and O-3 has recovered to levels similar to the beginning of the record. Our understanding of the causes of the longer-term changes is limited, although it appears that in the mid-latitudes of the northern hemisphere, controls on O-3 precursors have likely been a factor in the leveling off or decline from earlier O-3 increases. (C) 2012 Elsevier Ltd. All rights reserved.
C1 [Oltmans, S. J.] Univ Colorado, CIRES, Boulder, CO 80309 USA.
[Oltmans, S. J.; Harris, J. M.; Johnson, B. J.] NOAA Earth Syst Res Lab, Global Monitoring Div, Boulder, CO USA.
[Lefohn, A. S.] ASL & Associates, Helena, MT USA.
[Scheel, H. E.] KIT IMK IFU, Garmisch Partenkirchen, Germany.
[Galbally, I.] CSIRO, Ctr Australian Weather & Climate Res, Aspendale, Vic, Australia.
[Tarasick, D. W.; Davies, J.] Environm Canada, Toronto, ON, Canada.
[Nichol, S.] NIWA, Wellington, New Zealand.
[Schmidlin, F.] NASA, Wallops Isl, VA USA.
[Cuevas, E.; Redondas, A.] AEMET, Izana Atmospher Res Ctr, Tenerife, Canary Islands, Spain.
[Naoe, H.; Nakano, T.; Kawasato, T.] Japan Meteorol Agcy, Tokyo, Japan.
RP Oltmans, SJ (reprint author), Univ Colorado, CIRES, Boulder, CO 80309 USA.
EM Samuel.J.Oltmans@noaa.gov
RI Garmisch-Pa, Ifu/H-9902-2014; Galbally, Ian/E-5852-2011; Redondas,
Alberto/L-9299-2015; Cuevas, Emilio/L-2109-2013
OI Tarasick, David/0000-0001-9869-0692; Galbally, Ian/0000-0003-2383-1360;
Redondas, Alberto/0000-0002-4826-6823; Cuevas,
Emilio/0000-0003-1843-8302
NR 57
TC 61
Z9 65
U1 6
U2 106
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 1352-2310
J9 ATMOS ENVIRON
JI Atmos. Environ.
PD MAR
PY 2013
VL 67
BP 331
EP 351
DI 10.1016/j.atmosenv.2012.10.057
PG 21
WC Environmental Sciences; Meteorology & Atmospheric Sciences
SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences
GA 093EA
UT WOS:000315173300036
ER
PT J
AU Mielke, SP
Kiang, NY
Blankenship, RE
Mauzerall, D
AF Mielke, Steven P.
Kiang, Nancy Y.
Blankenship, Robert E.
Mauzerall, David
TI Photosystem trap energies and spectrally-dependent energy-storage
efficiencies in the Chl d-utilizing cyanobacterium, Acaryochloris marina
SO BIOCHIMICA ET BIOPHYSICA ACTA-BIOENERGETICS
LA English
DT Article
DE Acaryochloris marina; Chlorophyll d; Photosynthetic energy-storage;
Photosynthetic efficiency; Limits of oxygenic photosynthesis;
Photoacoustics
ID PHOTOSYNTHETIC REACTION CENTERS; D-DOMINATED CYANOBACTERIUM;
ELECTRON-TRANSFER REACTIONS; II CORE COMPLEXES; CHLOROPHYLL-D;
SYNECHOCOCCUS-ELONGATUS; OXYGENIC PHOTOSYNTHESIS; VOLUME CHANGE; WATER
OXIDATION; OPTICAL-SPECTRA
AB Acaryochloris marina is the only species known to utilize chlorophyll (Chl) d as a principal photopigment. The peak absorption wavelength of Chl d is redshifted approximate to 40 nm in vivo relative to Chl a, enabling this cyanobacterium to perform oxygenic phototrophy in niche environments enhanced in far-red light. We present measurements of the in vivo energy-storage (E-S) efficiency of photosynthesis in A. marina, obtained using pulsed photoacoustics (PA) over a 90-nm range of excitation wavelengths in the red and far-red. Together with modeling results, these measurements provide the first direct observation of the trap energies of PSI and PSII, and also the photosystem-specific contributions to the total E-S efficiency. We find the maximum observed efficiency in A. marina (40 +/- 1% at 735 nm) is higher than in the Chl a cyanobacterium Synechococcus leopoliensis (35 +/- 1% at 690 nm). The efficiency at peak absorption wavelength is also higher in A. marina (36 +/- 1% at 710 nm vs. 31 +/- 1% at 670 nm). In both species, the trap efficiencies are approximate to 40% (PSI) and approximate to 30% (PSII). The PSI trap in A. marina is found to lie at 740 +/- 5 nm, in agreement with the value inferred from spectroscopic methods. The best fit of the model to the PA data identifies the PSII trap at 723 +/- 3 nm, supporting the view that the primary electron-donor is Chl d, probably at the accessory (Chl(D1)) site. A decrease in efficiency beyond the trap wavelength, consistent with uphill energy transfer, is clearly observed and fit by the model. These results demonstrate that the E-S efficiency in A. marina is not thermodynamically limited, suggesting that oxygenic photosynthesis is viable in even redder light environments. (C) 2012 Elsevier B.V. All rights reserved.
C1 [Mielke, Steven P.; Mauzerall, David] Rockefeller Univ, Lab Photobiol, New York, NY 10065 USA.
[Kiang, Nancy Y.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
[Blankenship, Robert E.] Washington Univ, Dept Biol, St Louis, MO 63130 USA.
[Blankenship, Robert E.] Washington Univ, Dept Chem, St Louis, MO 63130 USA.
RP Mielke, SP (reprint author), Rockefeller Univ, Lab Photobiol, New York, NY 10065 USA.
EM spmielke@gmail.com
FU NASA [NNX08AP62G]; NAI; National Aeronautics and Space Administration
through the NAI [NNA08CN87A]
FX We are grateful to Irena Zielinski-Large for technical support; Dr. Carl
Pitcher (NASA Astrobiology Institute [NAI]) and Prof. Victoria Meadows
(Virtual Planetary Laboratory Lead Team, NAI) for support by a NASA
Postdoctoral Program fellowship, NAI Director's Discretionary Fund
grants, and the National Aeronautics and Space Administration through
the NAI under Cooperative Agreement No. NNA08CN87A; and Prof. M. R.
Gunner and Dr. Minghui Dong for helpful discussions. REB also thanks the
Exobiology Program of NASA for support under grant number NNX08AP62G.
NR 60
TC 9
Z9 10
U1 1
U2 37
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0005-2728
J9 BBA-BIOENERGETICS
JI Biochim. Biophys. Acta-Bioenerg.
PD MAR
PY 2013
VL 1827
IS 3
BP 255
EP 265
DI 10.1016/j.bbabio.2012.11.002
PG 11
WC Biochemistry & Molecular Biology; Biophysics
SC Biochemistry & Molecular Biology; Biophysics
GA 094FS
UT WOS:000315249000004
PM 23159726
ER
PT J
AU Simpson, DG
AF Simpson, David G.
TI NASA COMPUTATIONAL CASE STUDY: THE FLIGHT OF FRIENDSHIP 7
SO COMPUTING IN SCIENCE & ENGINEERING
LA English
DT Editorial Material
AB In this case study, we study a method for computing the position of an Earth-orbiting spacecraft as a function of time. As an exercise, we compute the position of John Glenn's Mercury spacecraft Friendship 7 as it orbited the Earth during the third flight of NASA's Mercury program.
C1 [Simpson, David G.] NASA, Goddard Space Flight Ctr, Washington, DC 20546 USA.
[Simpson, David G.] Prince Georges Community Coll, Largo, MD USA.
RP Simpson, DG (reprint author), NASA, Goddard Space Flight Ctr, Washington, DC 20546 USA.
EM david.g.simpson@nasa.gov
NR 11
TC 0
Z9 0
U1 0
U2 1
PU IEEE COMPUTER SOC
PI LOS ALAMITOS
PA 10662 LOS VAQUEROS CIRCLE, PO BOX 3014, LOS ALAMITOS, CA 90720-1314 USA
SN 1521-9615
J9 COMPUT SCI ENG
JI Comput. Sci. Eng.
PD MAR-APR
PY 2013
VL 15
IS 2
BP 72
EP 78
PG 7
WC Computer Science, Interdisciplinary Applications
SC Computer Science
GA 092OD
UT WOS:000315131000011
ER
PT J
AU Sarti, P
Abbondanza, C
Legrand, J
Bruyninx, C
Vittuari, L
Ray, J
AF Sarti, Pierguido
Abbondanza, Claudio
Legrand, Juliette
Bruyninx, Carine
Vittuari, Luca
Ray, Jim
TI Intrasite motions and monument instabilities at Medicina ITRF
co-location site
SO GEOPHYSICAL JOURNAL INTERNATIONAL
LA English
DT Article
DE Time-series analysis; Reference systems; Space geodetic surveys;
Intraplate processes; Europe
ID RADIO TELESCOPE; TIME-SERIES; GRAVITY VARIATIONS; SURFACE MONUMENTS;
DISPLACEMENT; DEFORMATION; GPS; BOLOGNA; SYSTEMS; SERVICE
AB We process the total-station surveys performed at the ITRF co-location site Medicina (Northern Italy) over the decade (2001-2010) with the purpose of determining the extent of local intrasite motions and relating them to local geophysical processes, the geological setting and the design of the ground pillars. In addition, continuous observations acquired by two co-located GPS stations (MEDI and MSEL separated by approximate to 27 m) are analysed and their relative motion is cross-checked with the total-station results. The local ground control network extends over a small area (<100 x 100 m) but the results demonstrate significant anisotropic deformations with rates up to 1.6 mm a(-1), primarily horizontal, a value comparable to intraplate tectonic deformations.
The results derived from GPS and total-station observations are consistent and point to the presence of horizontal intrasite motions over very short distances possibly associated with varying environmental conditions in a very unfavourable local geological setting and unsuitable monument design, these latter being crucial aspects of the realization and maintenance of global permanent geodetic networks and the global terrestrial reference frame.
C1 [Sarti, Pierguido] Ist Nazl Astrofis INAF, Ist Radioastron IRA, I-40129 Bologna, Italy.
[Abbondanza, Claudio] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Legrand, Juliette; Bruyninx, Carine] Royal Observ Belgium, B-1180 Brussels, Belgium.
[Vittuari, Luca] Univ Bologna, DICAM, I-40136 Bologna, Italy.
[Ray, Jim] NOAA, Natl Geodet Survey, Silver Spring, MD 20910 USA.
RP Sarti, P (reprint author), Ist Nazl Astrofis INAF, Ist Radioastron IRA, Via P Gobetti 101, I-40129 Bologna, Italy.
EM p.sarti@ira.inaf.it
RI Sarti, Pierguido/D-2391-2009;
OI Sarti, Pierguido/0000-0003-1260-5587; Vittuari, Luca/0000-0002-9815-1004
NR 46
TC 5
Z9 5
U1 2
U2 7
PU OXFORD UNIV PRESS
PI OXFORD
PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND
SN 0956-540X
EI 1365-246X
J9 GEOPHYS J INT
JI Geophys. J. Int.
PD MAR
PY 2013
VL 192
IS 3
BP 1042
EP 1051
DI 10.1093/gji/ggs092
PG 10
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 091LP
UT WOS:000315051300012
ER
PT J
AU Ray, RD
Egbert, GD
AF Ray, Richard D.
Egbert, Gary D.
TI Reply to comments by S. R. Dickman on 'Fortnightly Earth rotation, ocean
tides and mantle anelasticity'
SO GEOPHYSICAL JOURNAL INTERNATIONAL
LA English
DT Editorial Material
DE Earth rotation variations; Tides and planetary waves; Mantle processes
ID LONG-PERIOD TIDES; EQUILIBRIUM; VARIABILITY; CONSTRAINTS; FIELD; MODEL
AB Dickman argues that our model of the Mf ocean tide is unrealistic and that this invalidates conclusions regarding mantle anelasticity. His evidence is based on comparison with his own ocean modelling experiments and on his physical intuition regarding near-equilibrium tides. That evidence is unconvincing. Simple physical arguments alone are enough to rebut his main points. Furthermore, we test here his suggestion of increasing bottom-friction dissipation by a factor of 100 over our preferred solution, and we show that this results in unacceptable polar motion and poor agreement with independent tide-gauge data. In contrast, tests against independent data lend support to the realism of our Mf tide model and give confidence that our estimates of mantle anelasticity are reliable within stated error bounds.
C1 [Ray, Richard D.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Egbert, Gary D.] Oregon State Univ, Coll Ocean & Atmospher Sci, Corvallis, OR 97331 USA.
RP Ray, RD (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
EM richard.ray@nasa.gov
RI Ray, Richard/D-1034-2012;
OI Egbert, Gary/0000-0003-1276-8538
NR 20
TC 0
Z9 0
U1 0
U2 11
PU OXFORD UNIV PRESS
PI OXFORD
PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND
SN 0956-540X
J9 GEOPHYS J INT
JI Geophys. J. Int.
PD MAR
PY 2013
VL 192
IS 3
BP 1055
EP 1058
DI 10.1093/gji/ggs078
PG 4
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 091LP
UT WOS:000315051300014
ER
PT J
AU Holzmann, GJ
AF Holzmann, Gerard J.
TI Landing a Spacecraft on Mars
SO IEEE SOFTWARE
LA English
DT Editorial Material
C1 CALTECH, NASA, Jet Prop Lab, Pasadena, CA 91125 USA.
RP Holzmann, GJ (reprint author), CALTECH, NASA, Jet Prop Lab, Pasadena, CA 91125 USA.
EM gholzmann@acm.org
NR 5
TC 8
Z9 8
U1 1
U2 9
PU IEEE COMPUTER SOC
PI LOS ALAMITOS
PA 10662 LOS VAQUEROS CIRCLE, PO BOX 3014, LOS ALAMITOS, CA 90720-1314 USA
SN 0740-7459
J9 IEEE SOFTWARE
JI IEEE Softw.
PD MAR-APR
PY 2013
VL 30
IS 2
BP 83
EP 86
PG 4
WC Computer Science, Software Engineering
SC Computer Science
GA 095GI
UT WOS:000315322300017
ER
PT J
AU Ferreira, RN
Chao, WC
AF Ferreira, Rosana Nieto
Chao, Winston C.
TI Aqua-planet simulations of the formation of the South Atlantic
convergence zone
SO INTERNATIONAL JOURNAL OF CLIMATOLOGY
LA English
DT Article
DE South American monsoon; cold fronts; SACZ
ID BRAZILIAN AMAZON BASIN; SCALE COMMON FEATURES; BAIU FRONTAL ZONE; WET
SEASON; SUMMER CIRCULATION; LAND-SURFACE; RAINY-SEASON; ANNUAL CYCLE;
LIFE-CYCLE; AMERICA
AB The impact of Amazon Basin convection and cold fronts on the formation and maintenance of the South Atlantic convergence zone (SACZ) is studied using aqua-planet simulations with a general circulation model. In the model, a circular patch of warm sea-surface temperature (SST) is used to mimic the effect of the Amazon Basin on South American monsoon convection. The aqua-planet simulations were designed to study the effect of the strength and latitude of Amazon Basin convection on the formation of the SACZ. The simulations indicate that the strength of the SACZ increases as the Amazon convection intensifies and is moved away from the equator. Of the two controls studied here, the latitude of the Amazon convection exerts the strongest effect on the strength of the SACZ. An analysis of the synoptic-scale variability in the simulations shows the importance of frontal systems in the formation of the aqua-planet SACZ. Composite time series of frontal systems that occurred in the simulations show that a robust SACZ occurs when fronts penetrate into the subtropics and become stationary there as they cross eastward of the longitude of the Amazon Basin. Moisture convergence associated with these frontal systems produces rainfall not along the model SACZ region and along a large portion of the northern model Amazon Basin. Simulations in which the warm SST patch was too weak or too close to the equator did not produce frontal systems that extended into the tropics and became stationary, and did not form a SACZ. In the model, the SACZ forms as Amazon Basin convection strengthens and migrates far enough southward to allow frontal systems to penetrate into the tropics and stall over South America. This result is in agreement with observations that the SACZ tends to form after the onset of the monsoon season in the Amazon Basin. Copyright (c) 2012 Royal Meteorological Society
C1 [Ferreira, Rosana Nieto] E Carolina Univ, Dept Geog, Greenville, NC 28590 USA.
[Chao, Winston C.] NASA, Goddard Space Flight Ctr, Global Modeling & Assimilat Off, Greenbelt, MD 20771 USA.
RP Ferreira, RN (reprint author), E Carolina Univ, Dept Geog, Greenville, NC 28590 USA.
EM ferreirar@ecu.edu
FU National Oceanic and Atmospheric Administration [NA07OAR4310495]; NASA
FX We wish to thank two anonymous reviewers for their thoughtful
contributions to this manuscript. Dr Rosana Nieto Ferreira thanks the
National Oceanic and Atmospheric Administration Climate and Global
Change Program Climate Prediction Program for the Americas for its
support of this research (Award Number: NA07OAR4310495). Dr Winston Chao
was supported by NASA's Modeling, Analysis, and Prediction Program.
NR 36
TC 3
Z9 3
U1 0
U2 9
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 0899-8418
J9 INT J CLIMATOL
JI Int. J. Climatol.
PD MAR
PY 2013
VL 33
IS 3
BP 615
EP 628
DI 10.1002/joc.3457
PG 14
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 089QZ
UT WOS:000314926400008
ER
EF