FN Thomson Reuters Web of Science™
VR 1.0
PT J
AU Arab-Sedze, M
Heggy, E
Bretar, F
Berveiller, D
Jacquemoud, S
AF Arab-Sedze, M.
Heggy, E.
Bretar, F.
Berveiller, D.
Jacquemoud, S.
TI Quantification of L-band InSAR coherence over volcanic areas using LiDAR
and in situ measurements
SO REMOTE SENSING OF ENVIRONMENT
LA English
DT Article
DE Radar coherence; L-band; LiDAR; Volcanic areas; Surface roughness; Radar
wave penetration; Vegetation density; Piton de la Fournaise
ID GROUND-PENETRATING RADAR; INTERFEROMETRIC RADAR; VEGETATION INDEXES;
FOURNAISE VOLCANO; REUNION-ISLAND; PINE FOREST; LASER; DECORRELATION;
SURFACE; PITON
AB Interferometric Synthetic Aperture Radar (InSAR) is a powerful tool to monitor large-scale ground deformation at active volcanoes. However, vegetation and pyroclastic deposits degrade the radar coherence and therefore the measurement of 3-D surface displacements. In this article, we explore the complementarity between ALOS-PALSAR coherence images, airborne LiDAR data and in situ measurements acquired over the Piton de La Fournaise volcano (Reunion Island, France) to determine the sources of errors that may affect repeat-pass InSAR measurements. We investigate three types of surfaces: terrains covered with vegetation, lava flows (a'a, pahoehoe or slabby pahoehoe lava flows) and pyroclastic deposits (lapilli). To explain the loss of coherence observed over the Dolomieu crater between 2008 and 2009, we first use laser altimetry data to map topographic variations. The LiDAR intensity, which depends on surface reflectance, also provides ancillary information about the potential sources of coherence loss. In addition, surface roughness and rock dielectric properties of each terrain have been determined in situ to better understand how electromagnetic waves interact with such media: rough and porous surfaces, such as the a'a lava flows, produce a higher coherence loss than smoother surfaces, such as the pahoehoe lava flows. Variations in dielectric properties suggest a higher penetration depth in pyroclasts than in lava flows at L-band frequency. Decorrelation over the lapilli is hence mainly caused by volumetric effects. Finally, a map of LAI (Leaf Area Index) produced using SPOT 5 imagery allows us to quantify the effect of vegetation density: radar coherence is negatively correlated with LAI and is unreliable for values higher than 7.5. (C) 2014 Elsevier Inc. All rights reserved.
C1 [Arab-Sedze, M.; Jacquemoud, S.] Univ Paris Diderot, Sorbonne Paris Cite, Inst Phys Globe Paris, UMR CNRS 7154, F-75013 Paris, France.
[Arab-Sedze, M.] Inst Natl Informat Geog & Forestiere, Lab MATIS, F-94160 St Mande, France.
[Heggy, E.] NASA, Jet Prop Lab, Pasadena, CA 91109 USA.
[Bretar, F.] Consulat Gen France Shanghai, Serv Sci & Technol, Shanghai 200001, Peoples R China.
[Berveiller, D.] Univ Paris 11, AgroParisTech, CNRS, Lab Ecol Systemat & Evolut ESE,UMR 8079, F-91405 Orsay, France.
RP Arab-Sedze, M (reprint author), Inst Phys Globe Paris, Batiment Lamarck A,Case 7071, F-75013 Paris, France.
EM sedze@ipgp.fr; essam.heggy@jpl.nasa.gov; frederic.bretar@ieee.org;
daniel.berveiller@u-psud.fr; jacquemoud@ipgp.fr
RI Jacquemoud, Stephane/F-8842-2010
FU CNES; National Aeronautics and Space Administration
FX This work was funded by the CNES Terre Ocean Surfaces Continentales
Atmosphere (TOSCA) program from 2011 to 2013 in the frame of the DEVOIR
(DEformation of active vegetated VOlcanos using Insar and lidaR)
project. The Institut national de l'information geographique et
forestiere kindly provided the LiDAR data. 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. We thank our colleagues from the Observatoire
Volcanologique du Piton de la Fournaise (OVPF) for their support during
the geophysical survey.
NR 63
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PI NEW YORK
PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA
SN 0034-4257
EI 1879-0704
J9 REMOTE SENS ENVIRON
JI Remote Sens. Environ.
PD SEP
PY 2014
VL 152
BP 202
EP 216
DI 10.1016/j.rse.2014.06.011
PG 15
WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic
Technology
SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science &
Photographic Technology
GA AR2CW
UT WOS:000343392200017
ER
PT J
AU Ramsey, E
Rangoonwala, A
Chi, ZH
Jones, CE
Bannister, T
AF Ramsey, Elijah, III
Rangoonwala, Arnina
Chi, Zhaohui
Jones, Cathleen E.
Bannister, Terri
TI Marsh Dieback, loss, and recovery mapped with satellite optical,
airborne polarimetric radar, and field data
SO REMOTE SENSING OF ENVIRONMENT
LA English
DT Article
DE Spartina alterniflora marsh dieback; Optical vegetation indexes; NASA
UAVSAR; Polarimetric synthetic aperture radar (PoISAR); Coastal wetlands
ID SPARTINA-ALTERNIFLORA DIEBACK; COAST SALT MARSHES; LEAF-AREA INDEX;
L-BAND; C-BAND; LOUISIANA; REFLECTANCE; VEGETATION; SAR; WETLAND
AB Landsat Thematic Mapper and Satellite Pour l'Observation de la Terre (SPOT) satellite based optical sensors, NASA Uninhabited Aerial Vehicle synthetic aperture radar (UAVSAR) polarimetric SAR (PolSAR), and field data captured the occurrence and the recovery of an undetected dieback that occurred between the summers of 2010, 2011, and 2012 in the Spartina alterniflora marshes of coastal Louisiana. Field measurements recorded the dramatic biomass decrease from 2010 to 2011 and a biomass recovery in 2012 dominated by a decrease of live biomass, and the loss of marsh as part of the dieback event. Based on an established relationship, the near-infrared/red vegetation index (VI) and site-specific measurements delineated a contiguous expanse of marsh dieback encompassing 6649.9 ha of 18,2923 ha of S. alterniflora marshes within the study region. PoISAR data were transformed to variables used in biophysical mapping, and of this variable suite, the cross-polarization HV (horizontal send and vertical receive) backscatter was the best single indicator of marsh dieback and recovery. HV backscatter exhibited substantial and significant changes over the dieback and recovery period, tracked measured biomass changes, and significantly correlated with the live/dead biomass ratio. Within the context of regional trends, both HV and VI indicators started higher in pre-dieback marshes and exhibited substantially and statistically higher variability from year to year than that exhibited in the non-dieback marshes. That distinct difference allowed the capturing of the S. altemiflora marsh dieback and recovery; however, these changes were incorporated in a regional trend exhibiting similar but more subtle biomass composition changes. Published by Elsevier Inc.
C1 [Ramsey, Elijah, III] US Geol Survey, Natl Wetlands Res Ctr, Lafayette, LA 70506 USA.
[Rangoonwala, Arnina] Five Rivers Serv LLC, Colorado Springs, CO 80918 USA.
[Chi, Zhaohui; Bannister, Terri] Univ Louisiana Lafayette, CESU, Lafayette, LA 70506 USA.
[Jones, Cathleen E.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Ramsey, E (reprint author), US Geol Survey, Natl Wetlands Res Ctr, 700 Cajundome Blvd, Lafayette, LA 70506 USA.
EM ramseye@usgs.gov
FU National Aeronautics Space Administration (NASA) [11-TE11-104];
collaboration with the Jet Propulsion Laboratory, California Institute
of Technology, under a contract with NASA
FX We thank Francis Fields Jr. of the Apache Louisiana Minerals LLC, a
subsidiary of Apache Corporation, for access to their properties. We
also thank Ryan Longhenry, Data Management Specialist, U.S. Geological
Survey (USGS), Earth Resources Observation and Science (EROS) Center and
Carolyn Gacke, contractor Science Applications International Corporation
at USGS EROS Center for the help and support in providing the SPOT
satellite data. We appreciate the help by Sijan Sapkota of the U.S.
Geological Survey for his assistance in developing statistical models.
We appreciate the review of the manuscript by John liames, Research
Biologist at U.S. Environmental Protection Agency, and Dirk Werle of
AERDE Environmental Research, Canada. We also thank the two anonymous
reviewers for their exhaustive, judicious and perceptive reviews.
Research was supported in part by National Aeronautics Space
Administration (NASA) grant #11-TE11-104 and was carried out in
collaboration with the Jet Propulsion Laboratory, California Institute
of Technology, under a contract with NASA. Any use of trade, firm, or
product names is for descriptive purposes only and does not imply
endorsement by the U.S. Government
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SN 0034-4257
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J9 REMOTE SENS ENVIRON
JI Remote Sens. Environ.
PD SEP
PY 2014
VL 152
BP 364
EP 374
DI 10.1016/j.rse.2014.07.002
PG 11
WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic
Technology
SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science &
Photographic Technology
GA AR2CW
UT WOS:000343392200029
ER
PT J
AU Joiner, J
Yoshida, Y
Vasilkov, A
Schaefer, K
Jung, M
Guanter, L
Zhang, Y
Garrity, S
Middleton, EM
Huemmrich, KF
Gu, L
Marchesini, LB
AF Joiner, J.
Yoshida, Y.
Vasilkov, Ap.
Schaefer, K.
Jung, M.
Guanter, L.
Zhang, Y.
Garrity, S.
Middleton, E. M.
Huemmrich, K. F.
Gu, L.
Marchesini, L. Belelli
TI The seasonal cycle of satellite chlorophyll fluorescence observations
and its relationship to vegetation phenology and ecosystem atmosphere
carbon exchange
SO REMOTE SENSING OF ENVIRONMENT
LA English
DT Article
DE Fluorescence; Vegetation; Fluorescence; Chlorophyll; GOME-2; Gross
primary productivity; Light-use efficiency; Flux tower; Growing season;
Carbon uptake period; Phenology
ID GROSS PRIMARY PRODUCTION; LIGHT-USE EFFICIENCY; DECIDUOUS BROADLEAF
FOREST; EDDY-COVARIANCE; UNITED-STATES; MODIS DATA; PHOTOSYNTHETIC
EFFICIENCY; RESPONSE PARAMETERS; TOWER MEASUREMENTS; FLUX MEASUREMENTS
AB Mapping of terrestrial chlorophyll fluorescence from space has shown potential for providing global measurements related to gross primary productivity (GPP). In particular, space-based fluorescence may provide information on the length of the carbon uptake period. Here, for the first time we test the ability of satellite fluorescence retrievals to track seasonal cycle of photosynthesis as estimated from a diverse set of tower gas exchange measurements from around the world. The satellite fluorescence retrievals are obtained using new observations near the 740 nm emission feature from the Global Ozone Monitoring Experiment 2 (GOME-2) instrument offering the highest temporal and spatial resolution of available global measurements. Because GOME-2 has a large ground footprint (similar to 40 x 80 km(2)) as compared with that of the flux towers and the GOME-2 data require averaging to reduce random errors, we additionally compare with seasonal cycles of upscaled GPP estimated from a machine learning approach averaged over the same temporal and spatial domain as the satellite data surrounding the tower locations. We also examine the seasonality of absorbed photosynthetically-active radiation (AFAR) estimated from satellite measurements. Finally, to assess whether global vegetation models may benefit from the satellite fluorescence retrievals through validation or additional constraints, we examine seasonal cycles of GPP as produced from an ensemble of vegetation models. Several of the data-driven models rely on satellite reflectance-based vegetation parameters to derive estimates of APAR that are used to compute GPP. For forested (especially deciduous broadleaf and mixed forests) and cropland sites, the GOME-2 fluorescence data track the spring onset and autumn shutoff of photosynthesis as delineated by the upscaled GPP estimates. In contrast the reflectance-based indicators and many of the models, particularly those driven by data, tend to overestimate the length of the photosynthetically-active period for these biomes. Satellite fluorescence measurements therefore show potential for improving the seasonal dependence of photosynthesis simulated by global models at similar spatial scales. (C) 2014 Elsevier Inc All rights reserved.
C1 [Joiner, J.; Middleton, E. M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Yoshida, Y.; Vasilkov, Ap.] Sci Syst & Applicat Inc, Lanham, MD USA.
[Schaefer, K.] Univ Colorado, Natl Snow & Ice Data Ctr, Boulder, CO 80309 USA.
[Jung, M.] Max Planck Inst Biogeochem, D-07745 Jena, Germany.
[Guanter, L.; Zhang, Y.] Free Univ Berlin, Berlin, Germany.
[Garrity, S.] Los Alamos Natl Lab, Los Alamos, NM 87544 USA.
[Huemmrich, K. F.] Univ Maryland Baltimore Cty, JCET, Baltimore, MD 21228 USA.
[Gu, L.] Oak Ridge Natl Lab, Div Environm Sci, Oak Ridge, TN 37831 USA.
[Marchesini, L. Belelli] Vrije Univ Amsterdam, Amsterdam, Netherlands.
RP Garrity, S (reprint author), Los Alamos Natl Lab, Los Alamos, NM 87544 USA.
EM Joanna.joiner@nasa.gov
RI Guanter, Luis/I-1588-2015; Belelli Marchesini, Luca/M-3554-2014; Gu,
Lianhong/H-8241-2014;
OI Guanter, Luis/0000-0002-8389-5764; Belelli Marchesini,
Luca/0000-0001-8408-4675; Gu, Lianhong/0000-0001-5756-8738; Zhang,
Yongguang/0000-0001-8286-300X
FU NASA Carbon Cycle Science program [NNH1ODA001N]; U.S. Department of
Energy, Biological and Environmental Research, Terrestrial Carbon
Program [DEFG0204ER63917, DEFG0204ER63911]; CFCAS; NSERC; BIOCAP;
Environment Canada; NRCan; CarboEuropeIP; FAOGTOSTCO; iLEAPS; Max Planck
Institute for Biogeochemistry; National Science Foundation; University
of Tuscia; Wageningen University CALM Group; Universit Laval; U.S.
Department of Energy; National Science Foundation (NSF); U.S. Department
of Agriculture (USDA); U.S. Department of Energy (DOE); Biological and
Environmental Research Program (BER); U.S. DOE, through the Midwestern
Center of the National Institute for Global Environmental Change (NIGEC)
[DE-FC03-90ER61010]; BER [DE FG02-03ER63624, DE-FG03-01ER63278]; NOAA
[NA09OAR4310063]; NASA [NNX10AR63G, NNX11A008A]; NASA Terrestrial
Ecology Program [NNX08AI77G]; NSF Biocomplexity Program [EAR-0120630];
Australian Research Council FT [FT1110602]; [DP130101566]
FX Funding for this work was provided in part by the NASA Carbon Cycle
Science program (NNH1ODA001N). The authors gratefully acknowledge
EUMETSAT and the MODIS data processing team for making available the
GOME-2 and MODIS data sets, respectively, used here as well as the
algorithm development teams. We also thank James Collatz, Randy Kawa,
William Cook, Yen-Ben Cheng, Larry Corp, Petya Campbell, Qingyuan Zhang,
and Arlindo da Silva for helpful discussions. We are indebted to Philip
Durbin for assistance with the GOME-2 satellite data set. We also thank
Joshua Fisher and an anonymous reviewer for helpful comments that helped
to improve the paper.; This study uses eddy covariance data acquired by
the FLUXNET community and in particular by the following networks:
AmeriFlux (U.S. Department of Energy, Biological and Environmental
Research, Terrestrial Carbon Program (DEFG0204ER63917 and
DEFG0204ER63911)) AfriFlux, CarboAfrica, CarboEuropelP, CarboItaly,
CarboMont, FluxnetCanada (supported by the CFCAS, NSERC, BIOCAP,
Environment Canada, and NRCan), GreenGrass, KoFlux, LBA, NECC, OzFlux,
and USCCC. We acknowledge the financial support to the eddy covariance
data harmonization provided by the CarboEuropeIP, FAOGTOSTCO, iLEAPS,
Max Planck Institute for Biogeochemistry, National Science Foundation,
University of Tuscia, Wageningen University CALM Group (Climate change
and Adaptive Land and Water Management), Universit Laval and Environment
Canada and U.S. Department of Energy and the database development and
technical support from the Berkeley Water Center, Lawrence Berkeley
National Laboratory, Microsoft Research eScience, Oak Ridge National
Laboratory, University of California Berkeley, University of Virginia,
and South Dakota State University. Sites in the U.S. also acknowledge
support from the National Science Foundation (NSF), U.S. Department of
Agriculture (USDA), and the U.S. Department of Energy (DOE). Funding for
this research was also provided by the Biological and Environmental
Research Program (BER), U.S. DOE, through the Midwestern Center of the
National Institute for Global Environmental Change (NIGEC) under
Cooperative Agreements DE-FC03-90ER61010, and from the BER under
Cooperative Agreements DE FG02-03ER63624 and DE-FG03-01ER63278, NOAA
grant NA09OAR4310063, and NASA grants NNX10AR63G and NNX11A008A. Any
opinions, findings, and conclusions or recommendations expressed in this
publication are those of the authors and do not necessarily reflect the
views of the DOE. Access to the MMSF AmeriFlux site is provided by the
Indiana Department of Natural Resources, Division of Forestry. The
ZA-Kru site was supported by the NASA Terrestrial Ecology Program (Grant
# NNX08AI77G) and NSF Biocomplexity Program (Grant # EAR-0120630)
through grants to NPH. The OzFlux sites (AU-Wac, AU-Fog, AI-How) were
provided by Jason Beringer who was funded under an Australian Research
Council FT (FT1110602) and project support from DP130101566. Support for
collection and archiving was provided through the Australia Terrestrial
Ecosystem Research Network (TERN) (http://www.tem.org.au).
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SN 0034-4257
EI 1879-0704
J9 REMOTE SENS ENVIRON
JI Remote Sens. Environ.
PD SEP
PY 2014
VL 152
BP 375
EP 391
DI 10.1016/j.rse.2014.06.022
PG 17
WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic
Technology
SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science &
Photographic Technology
GA AR2CW
UT WOS:000343392200030
ER
PT J
AU Shuai, YM
Masek, JG
Gao, F
Schaaf, CB
He, T
AF Shuai, Yanmin
Masek, Jeffrey G.
Gao, Feng
Schaaf, Crystal B.
He, Tao
TI An approach for the long-term 30-m land surface snow-free albedo
retrieval from historic Landsat surface reflectance and MODIS-based a
priori anisotropy knowledge
SO REMOTE SENSING OF ENVIRONMENT
LA English
DT Article
DE Albedo algorithm; Landsat; MODIS BRDF; Forest disturbance
ID BIDIRECTIONAL REFLECTANCE; HEMISPHERICAL REFLECTANCE; DIRECTIONAL
REFLECTANCE; ATMOSPHERIC CORRECTION; PARAMETERIZATION SIB2; VEGETATION
CANOPIES; FOREST DISTURBANCE; NADIR REFLECTANCE; USE EFFICIENCY; BOREAL
FOREST
AB Land surface albedo has been recognized by the Global Terrestrial Observing System (GTOS) as an essential climate variable crucial for accurate modeling and monitoring of the Earth's radiative budget. While global climate studies can leverage albedo datasets from MODIS, VIIRS, and other coarse-resolution sensors, many applications in heterogeneous environments can benefit from higher-resolution albedo products derived from Landsat We previously developed a "MODIS-concurrent" approach for the 30-meter albedo estimation which relied on combining post-2000 Landsat data with MODIS Bidirectional Reflectance Distribution Function (BRDF) information. Here we present a "pre-MODIS era" approach to extend 30-m surface albedo generation in time back to the 1980s, through an a priori anisotropy Look-Up Table (LUT) built up from the high quality MCD43A BRDF estimates over representative homogenous regions. Each entry in the LUT reflects a unique combination of land cover, seasonality, terrain information, disturbance age and type, and Landsat optical spectral bands. An initial conceptual WT was created for the Pacific Northwest (PNW) of the United-States and provides BRDF shapes estimated from MODIS observations for undisturbed and disturbed surface types (including recovery trajectories of burned areas and non-fire disturbances). By accepting the assumption of a generally invariant BRDF shape for similar land surface structures as a priori information, spectral white-sky and black-sky albedos are derived through albedo-to-nadir reflectance ratios as a bridge between the Landsat and MODIS scale. A further narrow-to-broadband conversion based on radiative transfer simulations is adopted to produce broadband albedos at visible, near infrared, and shortwave regimes. We evaluate the accuracy of resultant Landsat albedo using available field measurements at forested AmeriFlux stations in the PNW region, and examine the consistency of the surface albedo generated by this approach respectively with that from the "concurrent" approach and the coincident MODIS operational surface albedo products. Using the tower measurements as reference, the derived Landsat 30-m snow-free shortwave broadband albedo yields an absolute accuracy of 0.02 with a root mean square error less than 0.016 and a bias of no more than 0.007. A further cross-comparison over individual scenes shows that the retrieved white sky shortwave albedo from the "pre-MODIS era" LUT approach is highly consistent (R-2 = 0.988, the scene-averaged low RMSE = 0.009 and bias = -0.005) with that generated by the earlier "concurrent" approach. The Landsat albedo also exhibits more detailed landscape texture and a wider dynamic range of albedo values than the coincident 500-m MODIS operational products (MCD43A3), especially in the heterogeneous regions. Collectively, the "pre-MODIS" LUT and "concurrent" approaches provide a practical way to retrieve long-term Landsat albedo from the historic Landsat archives as far back as the 19805, as well as the current Landsat-8 mission, and thus support investigations into the evolution of the albedo of terrestrial biomes at fine resolution. (C) 2014 Elsevier Inc. All rights reserved.
C1 [Shuai, Yanmin] Earth Resources Technol Inc, NASA, GSFC, Biospher Sci Lab, Greenbelt, MD 20771 USA.
[Masek, Jeffrey G.] NASA, Goddard Space Flight Ctr, Biospher Sci Lab, Greenbelt, MD 20771 USA.
[Gao, Feng] USDA ARS, Hydrol & Remote Sensing Lab, Beltsville, MD 20705 USA.
[Schaaf, Crystal B.] Univ Massachusetts, Sch Environm, Boston, MA 02125 USA.
[He, Tao] Univ Maryland, Dept Geog Sci, College Pk, MD 20742 USA.
RP Shuai, YM (reprint author), Earth Resources Technol Inc, NASA, GSFC, Biospher Sci Lab, Code 618, Greenbelt, MD 20771 USA.
EM shuaiym@gmail.com
RI Masek, Jeffrey/D-7673-2012; He, Tao/H-5130-2012
OI He, Tao/0000-0003-2079-7988
FU NASA Terrestrial Ecology Program via a "Science of Terra/Aqua"
[NNX11AG53G]; U.S. Geological Survey (USGS) [G12PC00072]; MODIS team
under NASA [NNX12AL38G]
FX This study was supported by the NASA Terrestrial Ecology Program via a
"Science of Terra/Aqua" grant (#NNX11AG53G) and partly by the U.S.
Geological Survey (USGS) Landsat science team grant (G12PC00072). The
authors would like to thank AmeriFlux network for providing ground data,
the extra help on ground details from Drs. Beverly E. Law, Christoph
Thomas, William J. Massman, Sean Burns, and Tilden P. Meyers. We thank
the LEDAPS project and USGS for providing Landsat surface reflectance,
Dr. Zhuosen Wang and the entire MODIS team under NASA grant NNX12AL38G
for the generation of operational MCD43A (V005), the Multi-Resolution
Land Characteristics (MRLC) consortium to provide NLCD 2006 dataset, the
USDA forest service-RSAC and USGS-EROS for the publish of annual MTBS
dataset, and Jet Propulsion Laboratory for the open of SRTM data as well
University of Maryland for the further process on SRTM and the
generation of NAFD data.
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SN 0034-4257
EI 1879-0704
J9 REMOTE SENS ENVIRON
JI Remote Sens. Environ.
PD SEP
PY 2014
VL 152
BP 467
EP 479
DI 10.1016/j.rse.2014.07.009
PG 13
WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic
Technology
SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science &
Photographic Technology
GA AR2CW
UT WOS:000343392200035
ER
PT J
AU Mannino, A
Novak, MG
Hooker, SB
Hyde, K
Aurin, D
AF Mannino, Antonio
Novak, Michael G.
Hooker, Stanford B.
Hyde, Kimberly
Aurin, Dirk
TI Algorithm development and validation of CDOM properties for estuarine
and continental shelf waters along the northeastern U.S. coast
SO REMOTE SENSING OF ENVIRONMENT
LA English
DT Article
DE CDOM; MODIS; SeaWiFS; Chesapeake Bay; Ocean; Remote sensing; Ocean
color; Continental shelf; Middle Atlantic Bight; Gulf of Maine; Georges
Bank
ID DISSOLVED ORGANIC-MATTER; INHERENT OPTICAL-PROPERTIES; MIDDLE ATLANTIC
BIGHT; ABSORPTION SPECTRAL SLOPES; OCEAN COLOR ALGORITHMS; CANADIAN
BEAUFORT SEA; GLOBAL DISTRIBUTION; MISSISSIPPI RIVER; CHESAPEAKE BAY;
CHLOROPHYLL-A
AB An extensive set of field measurements have been collected throughout the continental margin of the northeastern U.S. from 2004 to 2011 to develop and validate ocean color satellite algorithms for the retrieval of the absorption coefficient of chromophoric dissolved organic matter (a(CDOM)) and CDOM spectral slopes for the 275:295 nm and 300:600 nm spectral range (S-275:295 and S-300:600). Remote sensing reflectance (R-rs) measurements computed from in-water radiometry profiles along with a(CDOM)(lambda) data are applied to develop several types of algorithms for the SeaWiFS and MODIS-Aqua ocean color satellite sensors, which involve least squares linear regression of a(CDOM)(X) with (1)R-rs band ratios, (2) quasi-analytical algorithm-based (QAA-based) products of total absorption coefficients, (3) multiple R-rs bands within a multiple linear regression (MLR) analysis, and (4) diffuse attenuation coefficient (K-d). The relative error (mean absolute percent difference; MAPD) for the MLR retrievals of a(CDOM)(275), a(CDOM)(355), a(CDOM)(380), a(CDOM)(412) and a(CDOM)(443) for our study region range from 20.4 to 23.9% for MODIS-Aqua and 27.3-30% for SeaWiFS. Because of the narrower range of CDOM spectral slope values, the MAPD for the MLR S-275:295 and S-300:600 algorithms are much lower ranging from 9.9% and 9.1% for SeaWiFS, respectively, and 8.7% and 9.7% for MODIS, respectively. Multi-year, seasonal and spatial MODIS-Aqua and SeaWiFS distributions of Claw, S-275:295 and S-300:600 processed with these algorithms are consistent with field measurements and the processes that impact CDOM levels along the continental shelf of the northeastern U.S. Several satellite data processing factors correlate with higher uncertainty in satellite retrievals of a(CDOM), S-275:295 and S-300.600 within the coastal ocean, including solar zenith angle, sensor viewing angle, and atmospheric products applied for atmospheric corrections. Algorithms that include ultraviolet R-rs bands provide a better fit to field measurements than algorithms without the ultraviolet R-rs bands. This suggests that satellite sensors with ultraviolet capability could provide better retrievals of CDOM. Because of the strong correlations between CDOM parameters and DOM constituents in the coastal ocean, satellite observations of CDOM parameters can be applied to study the distributions, sources and sinks of DOM, which are relevant for understanding the carbon cycle, modeling the Earth system, and to discern how the Earth is changing. Published by Elsevier Inc.
C1 [Mannino, Antonio; Hooker, Stanford B.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Novak, Michael G.; Aurin, Dirk] NASA, Goddard Space Flight Ctr, SSAI Inc, Greenbelt, MD 20771 USA.
[Hyde, Kimberly] NOAA, Northeast Fisheries Serv Ctr, Narragansett, RI 02882 USA.
RP Mannino, A (reprint author), NASA, Goddard Space Flight Ctr, Mail Code 616-1, Greenbelt, MD 20771 USA.
EM antonio.mannino@nasa.gov
RI Hooker, Stanford/E-2162-2012; Mannino, Antonio/I-3633-2014
FU NASA programs; Ocean Biology and Biogeochemistry Program (Climate
Variability of the East Coast [CliVEC] project and
calibration/validation project); Biodiversity Program; New Investigator
Program and Interdisciplinary Science
FX Various NASA programs supported the work described in this publication
including the Ocean Biology and Biogeochemistry Program (Climate
Variability of the East Coast [CliVEC] project and
calibration/validation project), Biodiversity Program, New Investigator
Program and Interdisciplinary Science. We thank the captains and crews
of the RN Delaware II, RN Sharp, RN Gulf Challenger, RN Connecticut, and
RN Fay Slover. Our profound gratitude to Jerry Prezioso, Jon Hare, and
Harvey Walsh for accommodating our CliVEC project research on NOAA's
Northeast Marine Fisheries Service Ecosystem Monitoring (ECO-Mon)
cruises. Many thanks to Veronica Lance, Xiaoju Pan, Davide D'Alimonte,
Mary Russ, Katherine Filippino, Peter Bernhardt, Jean-Noel Druon, and
John Morrow for their assistance on the various research cruises that
contributed to this work. We thank Mike Twardowski for organizing and
leading the OBB-supported calibration/validation project and cruises in
the Hudson River-Estuary and New York Bight region. Ru Morrison kindly
invited our group to participate on cruises in the Gulf of Maine and
waters surrounding the Martha's Vineyard Coastal Observatory. Thanks to
Jay Austin, Eileen Hofmann and John Klinck for planning and/or
assistance with the Old Dominion University Chesapeake Bay mouth
hydrography transects and data access. We express our sincere gratitude
to Chuck McClain and three anonymous reviewers for providing insightful
comments on a prior draft of this manuscript that improved the final
version of this manuscript. Many thanks to the NASA Goddard Space Flight
Center Ocean Biology Processing Group for their efforts in providing
high quality MODIS and SeaWiFS satellite data products.
NR 98
TC 10
Z9 11
U1 1
U2 29
PU ELSEVIER SCIENCE INC
PI NEW YORK
PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA
SN 0034-4257
EI 1879-0704
J9 REMOTE SENS ENVIRON
JI Remote Sens. Environ.
PD SEP
PY 2014
VL 152
BP 576
EP 602
DI 10.1016/j.rse.2014.06.027
PG 27
WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic
Technology
SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science &
Photographic Technology
GA AR2CW
UT WOS:000343392200043
ER
PT J
AU Al-Yaari, A
Wigneron, JP
Ducharne, A
Kerr, YH
Wagner, W
De Lannoy, G
Reichle, R
Al Bitar, A
Dorigo, W
Richaume, P
Mialon, A
AF Al-Yaari, A.
Wigneron, J. -P.
Ducharne, A.
Kerr, Y. H.
Wagner, W.
De lannoy, G.
Reichle, R.
Al Bitar, A.
Dorigo, W.
Richaume, P.
Mialon, A.
TI Global-scale comparison of passive (SMOS) and active (ASCAT) satellite
based microwave soil moisture retrievals with soil moisture simulations
(MERRA-Land)
SO REMOTE SENSING OF ENVIRONMENT
LA English
DT Article
DE SMOS; ASCAT; MERRA-Land; Soil; Moisture; Global; Vegetation; LAI
ID AMSR-E; TRIPLE COLLOCATION; ERS SCATTEROMETER; IN-SITU; MODEL;
VALIDATION; PRODUCTS; ASSIMILATION; MISSION; CALIBRATION
AB Global surface soil moisture (SSM) datasets are being produced based on active and passive microwave satellite observations and simulations from land surface models (LSM). This study investigates the consistency of two global satellite-based SSM datasets based on microwave remote sensing observations from the passive Soil Moisture and Ocean Salinity (SMOS; SMOSL3 version 2.5) and the active Advanced Scatterometer (ASCAT; version TU-Wien-WARP 5.5) with respect to LSM SSM from the MERRA-Land data product. The relationship between the global-scale SSM products was studied during the 2010-2012 period using (1) a time series statistics (considering both original SSM data and anomalies), (2) a space time analysis using Hovmoller diagrams, and (3) a triple collocation error model. The SMOSL3 and ASCAT retrievals are consistent with the temporal dynamics of modeled SSM (correlation R > 0.70 for original SSM) in the transition zones between wet and dry climates, including the Sahel, the Indian subcontinent, the Great Plains of North America, eastern Australia, and southeastern Brazil. Over relatively dense vegetation covers, a better consistency with MERRA-Land was obtained with ASCAT than with SMOSL3. However, it was found that ASCAT retrievals exhibit negative correlation versus MERRA-Land in some arid regions (e.g., the Sahara and the Arabian Peninsula). In terms of anomalies, SMOSL3 better captures the short term SSM variability of the reference dataset (MERRA-Land) than ASCAT over regions with limited radio frequency interference (RFI) effects (e.g., North America, South America, and Australia). The seasonal and latitudinal variations of SSM are relatively similar for the three products, although the MERRA-Land SSM values are generally higher and their seasonal amplitude is much lower than for SMOSL3 and ASCAT. Both SMOSL3 and ASCAT have relatively comparable triple collocation errors with similar spatial error patterns: (i) lowest errors in arid regions (e.g., Sahara and Arabian Peninsula), due to the very low natural variability of soil moisture in these areas, and Central America, and (ii) highest errors over most of the vegetated regions (e.g., northern Australia, India, central Asia, and South America). However, the ASCAT SSM product is prone to larger random errors in some regions (e.g., north-western Africa, Iran, and southern South Africa). Vegetation density was found to be a key factor to interpret the consistency with MERRA-Land between the two remotely sensed products (SMOSL3 and ASCAT) which provides complementary information on SSM. This study shows that both SMOS and ASCAT have thus a potential for data fusion into long-term data records. (C) 2014 British Geological Survey (c) NERC. Published by Elsevier Inc.
C1 [Al-Yaari, A.; Wigneron, J. -P.] INRA, UMR ISPA 1391, F-33140 Villenave Dornon, France.
[Al-Yaari, A.; Ducharne, A.] Univ Paris 06, CNRS, UMR METIS 7619, Paris, France.
[Al-Yaari, A.] Thamar Univ, Fac Sci Appl, Dept Geol, Thamar, Yemen.
[Kerr, Y. H.; Al Bitar, A.; Richaume, P.; Mialon, A.] Univ Toulouse 3, CNRS, CNES, IRD,UMR Ctr Etudes Spatiales BIOsphere CESBIO 51, F-31062 Toulouse, France.
[Wagner, W.; Dorigo, W.] Vienna Univ Technol, Dept Geodesy & Geoinformat, A-1040 Vienna, Austria.
[De lannoy, G.; Reichle, R.] NASA, Goddard Space Flight Ctr, Global Modeling & Assimilat Off Code 610 1, Greenbelt, MD 20771 USA.
RP Wigneron, JP (reprint author), INRA, UMR ISPA 1391, F-33140 Villenave Dornon, France.
EM wigneron@bordeaux.inra.fr
RI Reichle, Rolf/E-1419-2012; Al-Yaari, Amen/B-1444-2016;
OI Al-Yaari, Amen/0000-0001-7530-6088; Wagner,
Wolfgang/0000-0001-7704-6857; Al Bitar, Ahmad/0000-0002-1756-1096
FU TOSCA (Terre Ocean Surfaces Continentales et Atmosphere) CNES program;
Islamic Development Bank (IDB); NASA Soil Moisture Active Passive
mission
FX This research work was funded by the TOSCA (Terre Ocean Surfaces
Continentales et Atmosphere) CNES program and the Islamic Development
Bank (IDB). Gabrielle De Lannoy and Rolf Reichle were supported by the
NASA Soil Moisture Active Passive mission. The authors acknowledge CATDS
for the SMOSL3 dataset (http://catds.ifremer.fr) and the Vienna
University of Technology (TU-WIEN) for the ASCAT product. SMOS team at
CESBIO is thanked for fruitful discussions. Mr Christophe Moisy provided
valuable technical assistance.
NR 80
TC 38
Z9 39
U1 5
U2 53
PU ELSEVIER SCIENCE INC
PI NEW YORK
PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA
SN 0034-4257
EI 1879-0704
J9 REMOTE SENS ENVIRON
JI Remote Sens. Environ.
PD SEP
PY 2014
VL 152
BP 614
EP 626
DI 10.1016/j.rse.2014.07.013
PG 13
WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic
Technology
SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science &
Photographic Technology
GA AR2CW
UT WOS:000343392200045
ER
PT J
AU Franch, B
Vermote, EF
Claverie, M
AF Franch, B.
Vermote, E. F.
Claverie, M.
TI Intercomparison of Landsat albedo retrieval techniques and evaluation
against in situ measurements across the US SURFRAD network
SO REMOTE SENSING OF ENVIRONMENT
LA English
DT Article
DE Surface albedo; BRDF; Landsat; MODIS
ID BROAD-BAND ALBEDO; BIDIRECTIONAL REFLECTANCE; SURFACE ALBEDO;
CLIMATE-CHANGE; MODIS DATA; FEEDBACKS; VARIABILITY; VALIDATION; IMPACTS;
FORESTS
AB Surface albedo is an essential parameter not only for developing climate models, but also for most energy balance studies. While climate models are usually applied at coarse resolution, the energy balance studies, which are mainly focused on agricultural applications, require a high spatial resolution. In this context Landsat is one of the most used remote sensing sensors.
The albedo, estimated through the angular integration of the Bidirectional Reflectance Distribution Function (BRDF), requires an appropriate angular sampling of the surface. However, Landsat sampling characteristics, with nearly constant observation geometry and low illumination variation, prevent from deriving a surface albedo product.
In this paper we present an algorithm to derive a Landsat surface albedo based on the BRDF parameters estimated from the MODerate Resolution Imaging Spectroradiometer (MODIS) Climate Modeling Grid (CMG) surface reflectance product (M{O,Y}D09) using the VJB method (Vermote, Justice, & Breon, 2009). We base our method on Landsat unsupervised classification to disaggregate the BRDF parameters to the Landsat spatial resolution. We tested the proposed algorithm over five different sites of the US Surface Radiation (SURFRAD) network and inter-compare our results with Shuai, Masek, Gao, and Schaaf (2011) method, which also provides Landsat albedo. The results show that with the proposed method we can derive the surface albedo with a Root Mean Square Error (RMSE) of 0.015 (7%). This result supposes an improvement of 5% in the RMSE compared to Shuai et al.'s (2011) method (with a RMSE of 0.024, 12%) that is mainly determined by the correction of the negative bias (lower retrieved albedo than in situ data). (C) 2014 Elsevier Inc. All rights reserved.
C1 [Franch, B.; Claverie, M.] Univ Maryland, Dept Geog Sci, College Pk, MD 20742 USA.
[Franch, B.; Vermote, E. F.; Claverie, M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Franch, B (reprint author), NASA, Goddard Space Flight Ctr, Dept Geog Sci, Terr Informat Syst Lab, Mail Code 619,Bldg 32,Room N148A, Greenbelt, MD 20771 USA.
EM belen.franchgras@nasa.gov
NR 40
TC 11
Z9 11
U1 3
U2 24
PU ELSEVIER SCIENCE INC
PI NEW YORK
PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA
SN 0034-4257
EI 1879-0704
J9 REMOTE SENS ENVIRON
JI Remote Sens. Environ.
PD SEP
PY 2014
VL 152
BP 627
EP 637
DI 10.1016/j.rse.2014.07.019
PG 11
WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic
Technology
SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science &
Photographic Technology
GA AR2CW
UT WOS:000343392200046
ER
PT J
AU Free, J
AF Free, James
TI Conversation with Optimist-in-chief
SO AEROSPACE AMERICA
LA English
DT Editorial Material
C1 NASA Glenn Res Ctr, Cleveland, OH 44135 USA.
RP Free, J (reprint author), NASA Glenn Res Ctr, Cleveland, OH 44135 USA.
NR 0
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 0740-722X
J9 AEROSPACE AM
JI Aerosp. Am.
PD SEP
PY 2014
VL 52
IS 8
BP 18
EP 20
PG 3
WC Engineering, Aerospace
SC Engineering
GA AR0TC
UT WOS:000343283200012
ER
PT J
AU Roland, A
AF Roland, Alex
TI Arguments That Count: Physics, Computing, and Missile Defense, 1949-2012
SO ISIS
LA English
DT Book Review
C1 [Roland, Alex] Duke Univ, Durham, NC 27706 USA.
[Roland, Alex] Natl Aeronaut & Space Adm, Washington, DC USA.
RP Roland, A (reprint author), Duke Univ, Durham, NC 27706 USA.
NR 1
TC 0
Z9 0
U1 0
U2 2
PU UNIV CHICAGO PRESS
PI CHICAGO
PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA
SN 0021-1753
EI 1545-6994
J9 ISIS
JI Isis
PD SEP
PY 2014
VL 105
IS 3
BP 671
EP 672
PG 4
WC History & Philosophy Of Science
SC History & Philosophy of Science
GA AQ7PQ
UT WOS:000343011900063
ER
PT J
AU Ning, SA
Kroo, I
Aftosmis, MJ
Nemec, M
Kless, JE
AF Ning, S. Andrew
Kroo, Ilan
Aftosmis, Michael J.
Nemec, Marian
Kless, James E.
TI Extended Formation Flight at Transonic Speeds
SO JOURNAL OF AIRCRAFT
LA English
DT Article; Proceedings Paper
CT 29th AIAA Applied Aerodynamics Conference
CY JUN 27-30, 2011
CL Honolulu, HI
SP AIAA
ID BIRDS
AB Aircraft flown in formation can realize significant reductions in drag by flying in regions of wake upwash. However, most transports fly at transonic speeds where the impact of compressibility on formation flight is not well understood. This study uses an Euler solver to analyze the inviscid aerodynamic forces and moments of transonic wing/body configurations flying in a two-aircraft formation. Formations with large streamwise separation distances (10-50 wingspans) are considered. This work indicates that compressibility-related drag penalties in formation flight may be eliminated by slowing 2-3% below the nominal out-of-formation cruise Mach number, either at fixed lift coefficient or fixed altitude. The latter option has the additional benefit that the aerodynamic performance of the formation improves slightly at higher lift coefficients. Although optimal in-formation lift coefficients are not as high as those estimated by incompressible analyses, modest increases in altitude can yield further improvements in aerodynamic efficiency. Increasing the lateral separation of the aircraft allows for slightly higher cruise speeds in exchange for higher induced drag. For the configurations examined here, a 1-2% reduction in Mach number combined with a lateral spacing increase of 5% span (vertical spacing aligned with the vortex) achieves a total formation drag savings of about 10%.
C1 [Ning, S. Andrew; Kroo, Ilan] Stanford Univ, Dept Aeronaut & Astronaut, Stanford, CA 94305 USA.
[Aftosmis, Michael J.] NASA, Ames Res Ctr, Adv Supercomp Div, Moffett Field, CA 94035 USA.
[Nemec, Marian; Kless, James E.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
RP Ning, SA (reprint author), Stanford Univ, Dept Aeronaut & Astronaut, Stanford, CA 94305 USA.
EM andrewning@alumni.stanford.edu
OI Ning, Andrew/0000-0003-2190-823X
NR 25
TC 1
Z9 1
U1 0
U2 7
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 SEP-OCT
PY 2014
VL 51
IS 5
BP 1501
EP 1510
DI 10.2514/1.C032385
PG 10
WC Engineering, Aerospace
SC Engineering
GA AQ8MS
UT WOS:000343080200016
ER
PT J
AU Guruswamy, GP
AF Guruswamy, Guru P.
TI Frequency Domain Flutter Boundary Computations Using Navier-Stokes
Equations on Superclusters
SO JOURNAL OF AIRCRAFT
LA English
DT Article; Proceedings Paper
CT 12th AIAA Aviation Technology, Integration, and Operations (ATIO)
Conference / 14th AIAA/ISSMO Multidisciplinary Analysis and Optimization
Conference
CY SEP 17-19, 2012
CL Indianapolis, IN
SP AIAA, ISSMO
C1 NASA, Ames Res Ctr, Fundamental Modeling & Simulat Branch, Adv Supercomp Div, Moffett Field, CA 94035 USA.
RP Guruswamy, GP (reprint author), NASA, Ames Res Ctr, Fundamental Modeling & Simulat Branch, Adv Supercomp Div, Moffett Field, CA 94035 USA.
NR 12
TC 2
Z9 2
U1 0
U2 1
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 SEP-OCT
PY 2014
VL 51
IS 5
BP 1640
EP 1642
DI 10.2514/1.C032126
PG 3
WC Engineering, Aerospace
SC Engineering
GA AQ8MS
UT WOS:000343080200028
ER
PT J
AU DeHaven, S
Wincheski, R
Albin, S
AF DeHaven, Stanton
Wincheski, Russell
Albin, Sacharia
TI Anthracene Fibers Grown in a Microstructured Optical Fiber for X-ray
Detection
SO MATERIALS
LA English
DT Article
DE growth from melt; organic compounds; scintillating materials; optical
fiber devices
ID SINGLE-CRYSTALS; ORGANIC CRYSTALS; ELECTROLUMINESCENCE; PRESSURE;
SPECTRA
AB Anthracene fibers are grown inside a microstructured quartz matrix to form a multicore optical fiber for X-ray detection. A modified fiber growth method for single crystal anthracene from the melt via the Bridgman-Stockbarger technique is presented. The anthracene fiber is characterized by using spectrophotometry, Raman spectroscopy, and X-ray diffraction. These results show the anthracene grown in fiber has high purity and a crystal structure similar to anthracene grown from liquid, vapor, and melt techniques. As an X-ray detector, the output is 12%-16% efficient between the energy ranges of 40 and 10 keV. The effect of materials and fiber processing are discussed.
C1 [DeHaven, Stanton; Wincheski, Russell] NASA Langley Res Ctr, Hampton, VA 23681 USA.
[Albin, Sacharia] Norfolk State Univ, Dept Engn, Norfolk, VA 23504 USA.
[Albin, Sacharia] Norfolk State Univ, Ctr Biotechnol & Biomed Sci, Norfolk, VA 23504 USA.
RP DeHaven, S (reprint author), NASA Langley Res Ctr, Hampton, VA 23681 USA.
EM stanton.l.dehaven@nasa.gov; russell.a.wincheski@nasa.gov; salbin@nsu.edu
NR 38
TC 2
Z9 2
U1 2
U2 9
PU MDPI AG
PI BASEL
PA POSTFACH, CH-4005 BASEL, SWITZERLAND
SN 1996-1944
J9 MATERIALS
JI Materials
PD SEP
PY 2014
VL 7
IS 9
BP 6291
EP 6303
DI 10.3390/ma7096291
PG 13
WC Materials Science, Multidisciplinary
SC Materials Science
GA AQ8QS
UT WOS:000343095300014
ER
PT J
AU Westgate, JA
Pearce, NJG
Gatti, E
Achyuthan, H
AF Westgate, John A.
Pearce, Nicholas J. G.
Gatti, Emma
Achyuthan, Hema
TI Distinction between the Youngest Toba Tuff and Oldest Toba Tuff from
northern Sumatra based on the area density of spontaneous fission tracks
in their glass shards
SO QUATERNARY RESEARCH
LA English
DT Article
DE Volcanic glass shards; Spontaneous fission tracks; Partial track fading;
Toba tuffs; Acheulean artifacts; Sumatra; India
ID INDIAN SUBCONTINENT; PENINSULAR INDIA; TEPHRA BEDS; AGE; INDONESIA;
ERUPTION; SUPERERUPTION; SEDIMENTS; ASH
AB Determination of the area density of spontaneous fission tracks (rho(s)) in glass shards of Toba tephra is a reliable way to distinguish between the Youngest Toba Tuff (YTT) and the Oldest Toba Tuff (OTT). The rho(s) values for YTT, uncorrected for partial track fading, range from 70 to 181 tracks/cm(2) with a weighted mean of 108 5 tracks/cm(2), based on 15 samples. Corrected rho(s) values for YTT are in the range of 77-140 tracks/cm(2) with a weighted mean of 113 +/- 8 tracks/cm(2), within the range of uncorrected rho(s) values. No significant difference in rho(s) exists between YTT samples collected from marine and continental depositional settings. The uncorrected rho(s) for OTT is 1567 +/- 114 tracks/cm(2) so that confusion with YTT is unlikely.
The rho(s) values of the Toba tephra at Bori, Morgaon, and Gandhigram in northwestern India indicate a YTT identity, in agreement with geochemical data on their glass shards, the presence of multiple glass populations, and a glass fission-track age determination. Therefore, the view of others that OTT is present at these sites - and thereby indicates an early Pleistocene age for the associated Acheulean artifacts - is incorrect. (C) 2014 University of Washington. Published by Elsevier Inc All rights reserved.
C1 [Westgate, John A.] Univ Toronto, Dept Earth Sci, Toronto, ON M5S 3B1, Canada.
[Pearce, Nicholas J. G.] Aberystwyth Univ, Dept Geog & Earth Sci, Aberystwyth SY23 3DB, Dyfed, Wales.
[Gatti, Emma] CALTECH, NASA, Jet Prop Lab, Pasadena, CA 91106 USA.
[Achyuthan, Hema] Anna Univ, Dept Geol, Chennai 600025, Tamil Nadu, India.
RP Westgate, JA (reprint author), Univ Toronto, Dept Earth Sci, Toronto, ON M5S 3B1, Canada.
EM westgate@es.utoronto.ca
RI Pearce, Nicholas/B-5295-2009;
OI Pearce, Nicholas/0000-0003-3157-9564
FU Natural Sciences and Engineering Research Council of Canada
FX Funds provided by the Natural Sciences and Engineering Research Council
of Canada are gratefully acknowledged. We thank Craig Chesner (Eastern
Illinois University, U.S.A.) and Jinnappa Pattan (CSIR, National
Institute of Oceanography, Goa, India) for samples. Significant
improvements to the manuscript were made following reviews by M. D.
Petraglia (University of Oxford), J. Dodson (Associate Editor), and an
anonymous reviewer.
NR 34
TC 2
Z9 2
U1 11
U2 18
PU ACADEMIC PRESS INC ELSEVIER SCIENCE
PI SAN DIEGO
PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA
SN 0033-5894
EI 1096-0287
J9 QUATERNARY RES
JI Quat. Res.
PD SEP
PY 2014
VL 82
IS 2
BP 388
EP 393
DI 10.1016/j.yqres.2014.07.001
PG 6
WC Geography, Physical; Geosciences, Multidisciplinary
SC Physical Geography; Geology
GA AQ8LJ
UT WOS:000343076700009
ER
PT J
AU Montanaro, M
Lunsford, A
Tesfaye, Z
Wenny, B
Reuter, D
AF Montanaro, Matthew
Lunsford, Allen
Tesfaye, Zelalem
Wenny, Brian
Reuter, Dennis
TI Radiometric Calibration Methodology of the Landsat 8 Thermal Infrared
Sensor
SO REMOTE SENSING
LA English
DT Article
DE Landsat; TIRS; radiometric calibration
AB The science-focused mission of the Landsat 8 Thermal Infrared Sensor (TIRS) requires that it have an accurate radiometric calibration. A calibration methodology was developed to convert the raw output from the instrument into an accurate at-aperture radiance. The methodology is based on measurements obtained during component-level and instrument-level characterization testing. The radiometric accuracy from the pre-flight measurements was estimated to be approximately 0.7%. The calibration parameters determined pre-flight were updated during the post-launch checkout period by utilizing the on-board calibration sources and Earth scene data. These relative corrections were made to adjust for differences between the pre-flight and the on-orbit performance of the instrument, thereby correcting large striping artifacts observed in Earth imagery. Despite this calibration correction, banding artifacts (low frequency variation in the across-track direction) have been observed in certain uniform Earth scenes, but not in other uniform scenes. In addition, the absolute calibration performance determined from vicarious measurements have revealed a time-varying error to the absolute radiance reported by TIRS. These issues were determined to not be caused by the calibration process developed for the instrument. Instead, an investigation has revealed that stray light is affecting the recorded signal from the Earth. The varying optical stray light effect is an ongoing subject of evaluation and investigation, and a correction strategy is being devised that will be added to the calibration process.
C1 [Montanaro, Matthew; Tesfaye, Zelalem; Wenny, Brian] NASA, Goddard Space Flight Ctr, Sigma Space Corp, Greenbelt, MD 20771 USA.
[Lunsford, Allen] NASA, Goddard Space Flight Ctr, Catholic Univ Amer, Greenbelt, MD 20771 USA.
[Reuter, Dennis] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Montanaro, M (reprint author), NASA, Goddard Space Flight Ctr, Sigma Space Corp, 8800 Greenbelt Rd, Greenbelt, MD 20771 USA.
EM matthew.montanaro@nasa.gov; allen.w.lunsford@nasa.gov;
zelalem.tesfaye-1@nasa.gov; brian.n.wenny@nasa.gov;
dennis.c.reuter@nasa.gov
FU NASA [NNG09HP18C]
FX The work presented here was funded under NASA Contract NNG09HP18C.
NR 12
TC 12
Z9 12
U1 2
U2 15
PU MDPI AG
PI BASEL
PA POSTFACH, CH-4005 BASEL, SWITZERLAND
SN 2072-4292
J9 REMOTE SENS-BASEL
JI Remote Sens.
PD SEP
PY 2014
VL 6
IS 9
BP 8803
EP 8821
DI 10.3390/rs6098803
PG 19
WC Remote Sensing
SC Remote Sensing
GA AQ8QI
UT WOS:000343093800040
ER
PT J
AU Traore, AK
Ciais, P
Vuichard, N
MacBean, N
Dardel, C
Poulter, B
Piao, SL
Fisher, JB
Viovy, N
Jung, M
Myneni, R
AF Traore, Abdoul Khadre
Ciais, Philippe
Vuichard, Nicolas
MacBean, Natasha
Dardel, Cecile
Poulter, Benjamin
Piao, Shilong
Fisher, Joshua B.
Viovy, Nicolas
Jung, Martin
Myneni, Ranga
TI 1982-2010 Trends of Light Use Efficiency and Inherent Water Use
Efficiency in African vegetation: Sensitivity to Climate and Atmospheric
CO2 Concentrations
SO REMOTE SENSING
LA English
DT Article
DE inherent water use efficiency; light use efficiency; Africa; trend
analysis; atmospheric CO2 effect and climate effects on vegetation
ID PHOTOSYNTHETICALLY ACTIVE RADIATION; NET ECOSYSTEM EXCHANGE; TREE-RING
DELTA-C-13; CARBON-DIOXIDE; DIFFUSE-RADIATION; FAGUS-SYLVATICA; ARID
ECOSYSTEMS; SOLAR-RADIATION; PAST CENTURY; RAIN-FOREST
AB Light and water use by vegetation at the ecosystem level, are key components for understanding the carbon and water cycles particularly in regions with high climate variability and dry climates such as Africa. The objective of this study is to examine recent trends over the last 30 years in Light Use Efficiency (LUE) and inherent Water Use Efficiency (iWUE*) for the major biomes of Africa, including their sensitivities to climate and CO2. LUE and iWUE* trends are analyzed using a combination of NOAA-AVHRR NDVI3g and fAPAR3g, and a data-driven model of monthly evapotranspiration and Gross Primary Productivity (based on flux tower measurements and remote sensing fAPAR, yet with no flux tower data in Africa) and the ORCHIDEE (ORganizing Carbon and Hydrology In Dynamic EcosystEms) process-based land surface model driven by variable CO2 and two different gridded climate fields. The iWUE* data product increases by 10%-20% per decade during the 1982-2010 period over the northern savannas (due to positive trend of vegetation productivity) and the central African forest (due to positive trend of vapor pressure deficit). In contrast to the iWUE*, the LUE trends are not statistically significant. The process-based model simulations only show a positive linear trend in iWUE* and LUE over the central African forest. Additionally, factorial model simulations were conducted to attribute trends in iWUE and LUE to climate change and rising CO2 concentrations. We found that the increase of atmospheric CO2 by 52.8 ppm during the period of study explains 30%-50% of the increase in iWUE* and > 90% of the LUE trend over the central African forest. The modeled iWUE* trend exhibits a high sensitivity to the climate forcing and environmental conditions, whereas the LUE trend has a smaller sensitivity to the selected climate forcing.
C1 [Traore, Abdoul Khadre; Ciais, Philippe; Vuichard, Nicolas; MacBean, Natasha; Viovy, Nicolas] LSCE IPSL CEA CNRS UVQS, Lab Sci Climat & Environm, F-91191 Gif Sur Yvette, France.
[Dardel, Cecile] CNRS UPS IRD CNES, UMR 5563, Observ Midi Pyrenees, GET, F-31400 Toulouse, France.
[Poulter, Benjamin] Montana State Univ, Dept Ecol, Bozeman, MT 59717 USA.
[Piao, Shilong] Peking Univ, Coll Urban & Environm Sci, Dept Ecol, Beijing 100871, Peoples R China.
[Piao, Shilong] Peking Univ, Key Lab Earth Surface Proc, Minist Educ, Beijing 100871, Peoples R China.
[Fisher, Joshua B.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Jung, Martin] Max Planck Inst Biogeochem, D-52425 Jena, Germany.
[Myneni, Ranga] Boston Univ, Dept Earth & Environm, Boston, MA 02215 USA.
RP Traore, AK (reprint author), LSCE IPSL CEA CNRS UVQS, Lab Sci Climat & Environm, F-91191 Gif Sur Yvette, France.
EM traore@lsce.ipsl.fr; philippe.ciais@lsce.ipsl.fr;
nicolas.vuichard@lsce.ipsl.fr; Natasha.MacBean@lsce.ipsl.fr;
cecile.dardel@gmail.com; benjamin.poulter@montana.edu;
slpiao@pku.edu.cn; Joshua.B.Fisher@jpl.nasa.gov;
nicolas.viovy@lsce.ipsl.fr; mjung@bgc-jena.mpg.de;
ranga.myneni@gmail.com
RI Myneni, Ranga/F-5129-2012; MacBean, Natasha/L-2190-2015; Vuichard,
Nicolas/A-6629-2011;
OI MacBean, Natasha/0000-0001-6797-4836; Poulter,
Benjamin/0000-0002-9493-8600
FU European Commission under the 7th Framework Programme (FP7)
FX This work is supported by the ClimAfrica project funded by the European
Commission under the 7th Framework Programme (FP7). We are grateful to
the GIMMS group for sharing the NDVI3g data (we thank Zaichun Zhu and
Ranga B. Myneni). Through Martin Jung, we are thankful to the Department
Biogeochemical Integration at the Max Planck Institute for
Biogeochemistry for providing Monthly gross primary productivity and
evapotranspiration deduced from FLUXNET data from the "La-Thuile-2007"
synthesis effort.
NR 82
TC 6
Z9 6
U1 4
U2 50
PU MDPI AG
PI BASEL
PA POSTFACH, CH-4005 BASEL, SWITZERLAND
SN 2072-4292
J9 REMOTE SENS-BASEL
JI Remote Sens.
PD SEP
PY 2014
VL 6
IS 9
BP 8923
EP 8944
DI 10.3390/rs6098923
PG 22
WC Remote Sensing
SC Remote Sensing
GA AQ8QI
UT WOS:000343093800045
ER
PT J
AU Eom, BH
Penanen, K
Hahn, I
AF Eom, Byeong Ho
Penanen, Konstantin
Hahn, Inseob
TI A cryogen-free ultralow-field superconducting quantum interference
device magnetic resonance imaging system
SO REVIEW OF SCIENTIFIC INSTRUMENTS
LA English
DT Article
ID MICROTESLA MRI; SQUID; MEG
AB Magnetic resonance imaging (MRI) at microtesla fields using superconducting quantum interference device (SQUID) detection has previously been demonstrated, and advantages have been noted. Although the ultralow-field SQUID MRI technique would not need the heavy superconducting magnet of conventional MRI systems, liquid helium required to cool the low-temperature detector still places a significant burden on its operation. We have built a prototype cryocooler-based SQUID MRI system that does not require a cryogen. The SQUID detector and the superconducting gradiometer were cooled down to 3.7 K and 4.3 K, respectively. We describe the prototype design, characterization, a phantom image, and areas of further improvements needed to bring the imaging performance to parity with conventional MRI systems. (C) 2014 AIP Publishing LLC.
C1 [Eom, Byeong Ho; Penanen, Konstantin; Hahn, Inseob] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Hahn, I (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM ihahn@caltech.edu
FU National Aeronautics and Space Administration (NASA)
FX I.H. gives thanks to Professor D. Goodstein for his support at Caltech.
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 (NASA).
NR 19
TC 1
Z9 1
U1 2
U2 8
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
EI 1089-7623
J9 REV SCI INSTRUM
JI Rev. Sci. Instrum.
PD SEP
PY 2014
VL 85
IS 9
AR 094302
DI 10.1063/1.4895998
PG 9
WC Instruments & Instrumentation; Physics, Applied
SC Instruments & Instrumentation; Physics
GA AQ6HE
UT WOS:000342910500046
PM 25273745
ER
PT J
AU Giorgi, AP
Rovzar, C
Davis, KS
Fuller, T
Buermann, W
Saatchi, S
Smith, TB
Silveira, LF
Gillespie, TW
AF Giorgi, Ana Paula
Rovzar, Corey
Davis, Kelsey S.
Fuller, Trevon
Buermann, Wolfgang
Saatchi, Sassan
Smith, Thomas B.
Silveira, Luis Fabio
Gillespie, Thomas W.
TI Spatial conservation planning framework for assessing conservation
opportunities in the Atlantic Forest of Brazil
SO APPLIED GEOGRAPHY
LA English
DT Article
DE Brazil; Ecological niche models; Endemic birds; Environmental
management; Protected areas; Radar
ID BIODIVERSITY CONSERVATION; SPECIES DISTRIBUTIONS; PASSERINE BIRDS;
LANDSCAPE; AREAS; PRIORITIZATION; BIOGEOGRAPHY; CHALLENGES; CORRIDORS;
DIVERSITY
AB Historic rates of habitat change and growing exploitation of natural resources threaten avian biodiversity in the Brazilian Atlantic Forest, a global biodiversity hotspot. We implemented a twostage framework for conservation planning in the Atlantic Forest. First, we used ecological niche modeling to predict the distributions of 23 endemic bird species using 19 climatic metrics and 12 spectral and radar remote sensing metrics. Second, we utilized the principle of complementarity to prioritize new sites to augment the Atlantic Forest's existing reserves. The best predictors of bird distributions were precipitation metrics (the seasonality of rainfall) and radar remote sensing metrics (QSCAT). The existing protected areas do not include 10% of the habitat of each of the 23 endemic species. We propose a more economical set of protected areas by reducing the extent to which new sites duplicate the biodiversity content of existing protected areas. There is a high concordance between the proposed conservation areas that we designed using computerized algorithms and Important Bird Areas prioritized by BirdLife International. Insofar as deforestation in the Atlantic Forest is similar to land conversion in other biodiversity hotspots, our methodology is applicable to conservation efforts elsewhere in the world. (C) 2014 Elsevier Ltd. All rights reserved.
C1 [Giorgi, Ana Paula; Rovzar, Corey; Davis, Kelsey S.; Gillespie, Thomas W.] Univ Calif Los Angeles, Dept Geog, Los Angeles, CA 90095 USA.
[Giorgi, Ana Paula; Fuller, Trevon; Smith, Thomas B.] Univ Calif Los Angeles, Ctr Trop Res, Los Angeles, CA 90095 USA.
[Buermann, Wolfgang] Univ Leeds, Sch Earth & Environm, Leeds LS2 9JT, W Yorkshire, England.
[Saatchi, Sassan] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Silveira, Luis Fabio] Univ Sao Paulo, BR-13418900 Piracicaba, SP, Brazil.
RP Gillespie, TW (reprint author), Univ Calif Los Angeles, Dept Geog, Los Angeles, CA 90095 USA.
EM TG@GEOG.UCLA.EDU
RI Silveira, Luis/F-8337-2012
OI Silveira, Luis/0000-0003-2576-7657
NR 47
TC 0
Z9 0
U1 2
U2 26
PU ELSEVIER SCI LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND
SN 0143-6228
EI 1873-7730
J9 APPL GEOGR
JI Appl. Geogr.
PD SEP
PY 2014
VL 53
BP 369
EP 376
DI 10.1016/j.apgeog.2014.06.013
PG 8
WC Geography
SC Geography
GA AQ1GK
UT WOS:000342529700032
PM 28210009
ER
PT J
AU Dutta, P
Rathi, M
Zheng, N
Gao, Y
Yao, Y
Martinez, J
Ahrenkiel, P
Selvamanickam, V
AF Dutta, P.
Rathi, M.
Zheng, N.
Gao, Y.
Yao, Y.
Martinez, J.
Ahrenkiel, P.
Selvamanickam, V.
TI High mobility single-crystalline-like GaAs thin films on inexpensive
flexible metal substrates by metal-organic chemical vapor deposition
SO APPLIED PHYSICS LETTERS
LA English
DT Article
ID COATED CONDUCTORS; CELLS
AB We demonstrate heteroepitaxial growth of single-crystalline-like n and p-type doped GaAs thin films on inexpensive, flexible, and light-weight metal foils by metal-organic chemical vapor deposition. Single-crystalline-like Ge thin film on biaxially textured templates made by ion beam assisted deposition on metal foil served as the epitaxy enabling substrate for GaAs growth. The GaAs films exhibited strong (004) preferred orientation, sharp in-plane texture, low grain misorientation, strong photoluminescence, and a defect density of similar to 10(7) cm(-2). Furthermore, the GaAs films exhibited hole and electron mobilities as high as 66 and 300 cm(2)/V-s, respectively. High mobility single-crystalline-like GaAs thin films on inexpensive metal substrates can pave the path for roll-to-roll manufacturing of flexible III-V solar cells for the mainstream photovoltaics market. (C) 2014 AIP Publishing LLC.
C1 [Dutta, P.; Rathi, M.; Gao, Y.; Yao, Y.; Selvamanickam, V.] Univ Houston, Dept Mech Engn, Houston, TX 77204 USA.
[Zheng, N.; Ahrenkiel, P.] South Dakota Sch Mines & Technol, Dept Nanosci & Nanoengn, Rapid City, SD 57701 USA.
[Martinez, J.] NASA, Lyndon B Johnson Space Ctr, Mat Evaluat Lab, Houston, TX 77085 USA.
RP Dutta, P (reprint author), Univ Houston, Dept Mech Engn, Houston, TX 77204 USA.
EM pdutta2@central.uh.edu
NR 25
TC 10
Z9 10
U1 2
U2 30
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
EI 1077-3118
J9 APPL PHYS LETT
JI Appl. Phys. Lett.
PD SEP 1
PY 2014
VL 105
IS 9
AR 092104
DI 10.1063/1.4895388
PG 5
WC Physics, Applied
SC Physics
GA AQ4FX
UT WOS:000342749800022
ER
PT J
AU d'Abzac, FX
Czaja, AD
Beard, BL
Schauer, JJ
Johnson, CM
AF d'Abzac, Francois-Xavier
Czaja, Andrew D.
Beard, Brian L.
Schauer, James J.
Johnson, Clark M.
TI Iron Distribution in Size-Resolved Aerosols Generated by UV-Femtosecond
Laser Ablation: Influence of Cell Geometry and Implications for In Situ
Isotopic Determination by LA-MC-ICP-MS
SO GEOSTANDARDS AND GEOANALYTICAL RESEARCH
LA English
DT Article
DE femtosecond laser ablation; aerosols; isotopes; agglomeration; residence
time
ID PLASMA-MASS-SPECTROMETRY; FE ISOTOPES; ELEMENTAL FRACTIONATION; RATIO
DETERMINATION; 266 NM; PARTICLES; SULFIDES; GLASS; NANOSECOND;
METEORITES
AB The influence of ablation cell geometry (Frames single- and HelEx two-volume cells) and laser wavelength (198 and 266nm) on aerosols produced by femtosecond laser ablation (fs-LA) were evaluated. Morphologies, iron mass distribution (IMD) and Fe-56/Fe-54 ratios of particles generated from magnetite, pyrite, haematite and siderite were studied. The following two morphologies were identified: spherules (10-200nm) and agglomerates (5-10nm). Similarity in IMD and ablation rate at 198 and 266nm indicates similar ablation mechanisms. Fe-56/Fe-54 ratios increased with aerodynamic particle size as a result of kinetic fractionation during laser plasma plume expansion, cooling and aerosol condensation. The HelEx cell produces smaller particles with a larger range of Fe-56/Fe-54 ratios (1.85) than particles from the Frames cell (1.16 parts per thousand), but the bulk aerosol matches the bulk substrate for both cells, demonstrating stoichiometric fs-LA sampling. IMD differences are the result of faster wash out of the HelEx cell allowing less time for agglomeration of small, low- Fe-56 particles with larger, high- Fe-56 particles in the cell. Even with a shorter ablation time, half the total Fe ion intensity, and half the ablation volume, the HelEx cell produced Fe isotope determinations for magnetite that were as precise as the Frames cell, even when the latter included an aerosol-homogenising mixing chamber. The HelEx cell delivered a more constant stream of small particles to the ICP, producing a more stable Fe ion signal (0.7% vs. 1.5% RSE for Fe-56 in a forty-cycle single analysis), constant instrumental mass bias and thus a more precise measurement.
C1 [d'Abzac, Francois-Xavier; Czaja, Andrew D.; Beard, Brian L.; Johnson, Clark M.] Univ Wisconsin, Dept Geosci, Madison, WI 53706 USA.
[d'Abzac, Francois-Xavier; Czaja, Andrew D.; Beard, Brian L.; Johnson, Clark M.] Univ Wisconsin, NASA Astrobiol Inst, Madison, WI 53706 USA.
[Czaja, Andrew D.] Univ Cincinnati, Dept Geol, Cincinnati, OH 45221 USA.
[Czaja, Andrew D.] Univ Cincinnati, Dept Chem, Cincinnati, OH 45221 USA.
[Schauer, James J.] Univ Wisconsin, Environm Chem & Technol Program, Madison, WI 53706 USA.
RP d'Abzac, FX (reprint author), Univ Wisconsin, Dept Geosci, 1215W Dayton St, Madison, WI 53706 USA.
EM fxdabzac@gmail.com
FU NSF [DMR-1121288]; NASA; NASA Astrobiology Institute
FX The authors gratefully acknowledge use of facilities and instrumentation
supported by the NSF-funded University of Wisconsin Materials Research
Science and Engineering Center (DMR-1121288). This study was funded by
NSF and NASA grants to C.M.J. and B. L. B., including funding from the
NASA Astrobiology Institute. The anonymous reviewers are thanked for
their constructive comments.
NR 70
TC 7
Z9 7
U1 2
U2 33
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 1639-4488
EI 1751-908X
J9 GEOSTAND GEOANAL RES
JI Geostand. Geoanal. Res.
PD SEP
PY 2014
VL 38
IS 3
BP 293
EP 309
DI 10.1111/j.1751-908X.2014.00281.x
PG 17
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA AQ4HQ
UT WOS:000342754900005
ER
PT J
AU Westphal, AJ
Anderson, D
Butterworth, AL
Frank, DR
Lettieri, R
Marchant, W
Von Korff, J
Zevin, D
Ardizzone, A
Campanile, A
Capraro, M
Courtney, K
Criswell, MN
Crumpler, D
Cwik, R
Gray, FJ
Hudson, B
Imada, G
Karr, J
Wah, LLW
Mazzucato, M
Motta, PG
Rigamonti, C
Spencer, RC
Woodrough, SB
Santoni, IC
Sperry, G
Terry, JN
Wordsworth, N
Yahnke, T
Allen, C
Ansari, A
Bajt, S
Bastien, RK
Bassim, N
Bechtel, HA
Borg, J
Brenker, FE
Bridges, J
Brownlee, DE
Burchell, M
Burghammer, M
Changela, H
Cloetens, P
Davis, AM
Doll, R
Floss, C
Flynn, G
Gainsforth, Z
Grun, E
Heck, PR
Hillier, JK
Hoppe, P
Huth, J
Hvide, B
Kearsley, A
King, AJ
Lai, B
Leitner, J
Lemelle, L
Leroux, H
Leonard, A
Nittler, LR
Ogliore, R
Ong, WJ
Postberg, F
Price, MC
Sandford, SA
Tresseras, JAS
Schmitz, S
Schoonjans, T
Silversmit, G
Simionovici, AS
Sole, VA
Srama, R
Stephan, T
Sterken, VJ
Stodolna, J
Stroud, RM
Sutton, S
Trieloff, M
Tsou, P
Tsuchiyama, A
Tyliszczak, T
Vekemans, B
Vincze, L
Zolensky, ME
AF Westphal, Andrew J.
Anderson, David
Butterworth, Anna L.
Frank, David R.
Lettieri, Robert
Marchant, William
Von Korff, Joshua
Zevin, Daniel
Ardizzone, Augusto
Campanile, Antonella
Capraro, Michael
Courtney, Kevin
Criswell, Mitchell N., III
Crumpler, Dixon
Cwik, Robert
Gray, Fred Jacob
Hudson, Bruce
Imada, Guy
Karr, Joel
Wah, Lily Lau Wan
Mazzucato, Michele
Motta, Pier Giorgio
Rigamonti, Carlo
Spencer, Ronald C.
Woodrough, Stephens B.
Santoni, Irene Cimmino
Sperry, Gerry
Terry, Jean-Noel
Wordsworth, Naomi
Yahnke, Tom, Sr.
Allen, Carlton
Ansari, Asna
Bajt, Sasa
Bastien, Ron K.
Bassim, Nabil
Bechtel, Hans A.
Borg, Janet
Brenker, Frank E.
Bridges, John
Brownlee, Donald E.
Burchell, Mark
Burghammer, Manfred
Changela, Hitesh
Cloetens, Peter
Davis, Andrew M.
Doll, Ryan
Floss, Christine
Flynn, George
Gainsforth, Zack
Gruen, Eberhard
Heck, Philipp R.
Hillier, Jon K.
Hoppe, Peter
Huth, Joachim
Hvide, Brit
Kearsley, Anton
King, Ashley J.
Lai, Barry
Leitner, Jan
Lemelle, Laurence
Leroux, Hugues
Leonard, Ariel
Nittler, Larry R.
Ogliore, Ryan
Ong, Wei Ja
Postberg, Frank
Price, Mark C.
Sandford, Scott A.
Tresseras, Juan-Angel Sans
Schmitz, Sylvia
Schoonjans, Tom
Silversmit, Geert
Simionovici, Alexandre S.
Sole, Vicente A.
Srama, Ralf
Stephan, Thomas
Sterken, Veerle J.
Stodolna, Julien
Stroud, Rhonda M.
Sutton, Steven
Trieloff, Mario
Tsou, Peter
Tsuchiyama, Akira
Tyliszczak, Tolek
Vekemans, Bart
Vincze, Laszlo
Zolensky, Michael E.
TI Stardust Interstellar Preliminary Examination I: Identification of
tracks in aerogel
SO METEORITICS & PLANETARY SCIENCE
LA English
DT Article
AB Here, we report the identification of 69 tracks in approximately 250 cm(2) of aerogel collectors of the Stardust Interstellar Dust Collector. We identified these tracks through Stardust@home, a distributed internet-based virtual microscope and search engine, in which > 30,000 amateur scientists collectively performed >9 x 10(7) searches on approximately 10(6) fields of view. Using calibration images, we measured individual detection efficiency, and found that the individual detection efficiency for tracks > 2.5 mu m in diameter was >0.6, and was >0.75 for tracks >3 mu m in diameter. Because most fields of view were searched >30 times, these results could be combined to yield a theoretical detection efficiency near unity. The initial expectation was that interstellar dust would be captured at very high speed. The actual tracks discovered in the Stardust collector, however, were due to low-speed impacts, and were morphologically strongly distinct from the calibration images. As a result, the detection efficiency of these tracks was lower than detection efficiency of calibrations presented in training, testing, and ongoing calibration. Nevertheless, as calibration images based on low-speed impacts were added later in the project, detection efficiencies for low-speed tracks rose dramatically. We conclude that a massively distributed, calibrated search, with amateur collaborators, is an effective approach to the challenging problem of identification of tracks of hypervelocity projectiles captured in aerogel.
C1 [Westphal, Andrew J.; Anderson, David; Butterworth, Anna L.; Lettieri, Robert; Marchant, William; Von Korff, Joshua; Zevin, Daniel; Gainsforth, Zack; Stodolna, Julien] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
[Frank, David R.; Bastien, Ron K.] NASA JSC, ESCG, Houston, TX USA.
[Ardizzone, Augusto] Red Team, Palermo, Italy.
[Campanile, Antonella] Red Team, Reggio Emilia, Italy.
[Capraro, Michael] Red Team, Riverview, MI USA.
[Courtney, Kevin] Red Team, Ballwin, MO USA.
[Criswell, Mitchell N., III] Dog Star Observ, Red Team, Pearce, AZ USA.
[Crumpler, Dixon] Red Team, Durham, NC USA.
[Cwik, Robert] Red Team, Silver City, NM USA.
[Gray, Fred Jacob] Red Team, Hampton, SC USA.
[Hudson, Bruce] Red Team, Montreal, PQ, Canada.
[Imada, Guy] Red Team, Brookings, OR USA.
[Karr, Joel] Red Team, Kansas City, MO USA.
[Wah, Lily Lau Wan] Red Team, Singapore, Singapore.
[Mazzucato, Michele; Motta, Pier Giorgio] Red Team, Florence, Italy.
[Rigamonti, Carlo] Red Team, Moncalieri, Italy.
[Spencer, Ronald C.] Red Team, Leominster, MA USA.
[Woodrough, Stephens B.] Red Team, St Petersburg, FL USA.
[Santoni, Irene Cimmino] Red Team, Upper Saddle River, NJ USA.
[Sperry, Gerry] Red Team, Tacoma, WA USA.
[Terry, Jean-Noel] Red Team, Tarentaise, France.
[Wordsworth, Naomi] Red Team, Wycombe, South Buckingha, England.
[Yahnke, Tom, Sr.] Red Team, Louis, MO USA.
[Allen, Carlton; Zolensky, Michael E.] NASA JSC, ARES, Houston, TX USA.
[Ansari, Asna; Hvide, Brit] Field Museum Nat Hist, Robert A Pritzker Ctr Meteorit & Polar Studies, Chicago, IL 60605 USA.
[Bajt, Sasa] DESY, Hamburg, Germany.
[Bassim, Nabil; Stroud, Rhonda M.] Naval Res Lab, Mat Sci & Technol Div, Washington, DC USA.
[Bechtel, Hans A.; Tyliszczak, Tolek] Lawrence Berkeley Lab, Adv Light Source, Berkeley, CA USA.
[Borg, Janet] IAS Orsay, Orsay, France.
[Brenker, Frank E.; Schmitz, Sylvia] Goethe Univ, Geosci Inst, Frankfurt, Germany.
[Bridges, John] Univ Leicester, Space Res Ctr, Leicester, Leics, England.
[Brownlee, Donald E.] Univ Washington, Dept Astron, Seattle, WA 98195 USA.
[Burchell, Mark; Price, Mark C.] Univ Kent, Canterbury, Kent, England.
[Burghammer, Manfred; Cloetens, Peter; Tresseras, Juan-Angel Sans; Sole, Vicente A.] European Synchrotron Radiat Facil, F-38043 Grenoble, France.
[Changela, Hitesh] George Washington Univ, Washington, DC 20052 USA.
[Davis, Andrew M.; Stephan, Thomas] Univ Chicago, Chicago, IL 60637 USA.
[Doll, Ryan; Leonard, Ariel; Nittler, Larry R.; Ong, Wei Ja] Washington Univ, St Louis, MO USA.
[Flynn, George] SUNY Coll Plattsburgh, Plattsburgh, NY 12901 USA.
[Gruen, Eberhard] Max Planck Inst Kernphys, D-69117 Heidelberg, Germany.
[Heck, Philipp R.] Field Museum Nat Hist, Chicago, IL 60605 USA.
[Hillier, Jon K.; Postberg, Frank; Trieloff, Mario] Heidelberg Univ, Inst Geowissensch, Heidelberg, Germany.
[Hoppe, Peter; Huth, Joachim; Leitner, Jan] Max Planck Inst Chem, D-55128 Mainz, Germany.
[Kearsley, Anton] Nat Hist Museum, London SW7 5BD, England.
[King, Ashley J.] Univ Chicago, Chicago, IL 60637 USA.
[King, Ashley J.] Field Museum Nat Hist, Robert A Pritzker Ctr Meteorit & Polar Studies, Chicago, IL 60605 USA.
[Lai, Barry; Sutton, Steven] Argonne Natl Lab, Adv Photon Source, Chicago, IL USA.
[Lemelle, Laurence] Ecole Normale Super Lyon, F-69364 Lyon, France.
[Leroux, Hugues] Univ Lyon 1, F-69622 Villeurbanne, France.
[Nittler, Larry R.] Carnegie Inst Sci, Washington, DC USA.
[Ogliore, Ryan] Univ Hawaii Manoa, Honolulu, HI 96822 USA.
[Sandford, Scott A.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Schoonjans, Tom; Silversmit, Geert; Vekemans, Bart; Vincze, Laszlo] Univ Ghent, B-9000 Ghent, Belgium.
[Simionovici, Alexandre S.] Univ Grenoble, Observ Sci, Inst Sci Terre, Grenoble, France.
[Srama, Ralf; Sterken, Veerle J.] Univ Stuttgart, IRS, D-70174 Stuttgart, Germany.
[Sterken, Veerle J.] TU Braunschweig, IGEP, Braunschweig, Germany.
[Sterken, Veerle J.] MPIK, Heidelberg, Germany.
[Tsou, Peter] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Tsuchiyama, Akira] Osaka Univ, Osaka, Japan.
RP Westphal, AJ (reprint author), Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
EM westphal@ssl.berkeley.edu
RI Sans Tresserras, Juan Angel/J-9362-2014; Leitner, Jan/A-7391-2015;
Hoppe, Peter/B-3032-2015; Bajt, Sasa/G-2228-2010; Stroud,
Rhonda/C-5503-2008;
OI Sans Tresserras, Juan Angel/0000-0001-9047-3992; Leitner,
Jan/0000-0003-3655-6273; Hoppe, Peter/0000-0003-3681-050X; Stroud,
Rhonda/0000-0001-5242-8015; Burchell, Mark/0000-0002-2680-8943
FU NASA [NNX09AC36G, NNH11AQ61I]; Office of Science, Office of Basic Energy
Sciences, of the U.S. Department of Energy [DE-AC02-05CH11231]; U.S.
Department of Energy, Office of Science, Office of Basic Energy Sciences
[DE-AC02-98CH10886]
FX We thank Sean Brennan and Giles Graham for thoughtful comments, and John
Bradley for editorial handling. The ISPE consortium gratefully
acknowledges the NASA Discovery Program for Stardust, the fourth NASA
Discovery mission. AJW, ALB, ZG, RL, DZ, WM, and JVK were supported by
NASA grant NNX09AC36G. We thank Steve Boggs for astrophysical soft X-ray
spectra. RMS, HCG, and NDB were supported by NASA grant NNH11AQ61I. 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. Use of the National Synchrotron Light
Source, Brookhaven National Laboratory, was supported by the U.S.
Department of Energy, Office of Science, Office of Basic Energy
Sciences, under Contract No. DE-AC02-98CH10886.
NR 8
TC 12
Z9 12
U1 3
U2 31
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 1086-9379
EI 1945-5100
J9 METEORIT PLANET SCI
JI Meteorit. Planet. Sci.
PD SEP
PY 2014
VL 49
IS 9
SI SI
BP 1509
EP 1521
DI 10.1111/maps.12168
PG 13
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA AQ6HT
UT WOS:000342912100001
ER
PT J
AU Frank, DR
Westphal, AJ
Zolensky, ME
Gainsforth, Z
Butterworth, AL
Bastien, RK
Allen, C
Anderson, D
Ansari, A
Bajt, S
Bassim, N
Bechtel, HA
Borg, J
Brenker, FE
Bridges, J
Brownlee, DE
Burchell, M
Burghammer, M
Changela, H
Cloetens, P
Davis, AM
Doll, R
Floss, C
Flynn, G
Grun, E
Heck, PR
Hillier, JK
Hoppe, P
Hudson, B
Huth, J
Hvide, B
Kearsley, A
King, AJ
Lai, B
Leitner, J
Lemelle, L
Leroux, H
Leonard, A
Lettieri, R
Marchant, W
Nittler, LR
Ogliore, R
Ong, WJ
Postberg, F
Price, MC
Sandford, SA
Tresseras, JAS
Schmitz, S
Schoonjans, T
Silversmit, G
Simionovici, AS
Sole, VA
Srama, R
Stephan, T
Sterken, VJ
Stodolna, J
Stroud, RM
Sutton, S
Trieloff, M
Tsou, P
Tsuchiyama, A
Tyliszczak, T
Vekemans, B
Vincze, L
Von Korff, J
Wordsworth, N
Zevin, D
AF Frank, David R.
Westphal, Andrew J.
Zolensky, Michael E.
Gainsforth, Zack
Butterworth, Anna L.
Bastien, Ronald K.
Allen, Carlton
Anderson, David
Ansari, Asna
Bajt, Sasa
Bassim, Nabil
Bechtel, Hans A.
Borg, Janet
Brenker, Frank E.
Bridges, John
Brownlee, Donald E.
Burchell, Mark
Burghammer, Manfred
Changela, Hitesh
Cloetens, Peter
Davis, Andrew M.
Doll, Ryan
Floss, Christine
Flynn, George
Gruen, Eberhard
Heck, Philipp R.
Hillier, Jon K.
Hoppe, Peter
Hudson, Bruce
Huth, Joachim
Hvide, Brit
Kearsley, Anton
King, Ashley J.
Lai, Barry
Leitner, Jan
Lemelle, Laurence
Leroux, Hugues
Leonard, Ariel
Lettieri, Robert
Marchant, William
Nittler, Larry R.
Ogliore, Ryan
Ong, Wei Ja
Postberg, Frank
Price, Mark C.
Sandford, Scott A.
Tresseras, Juan-Angel Sans
Schmitz, Sylvia
Schoonjans, Tom
Silversmit, Geert
Simionovici, Alexandre S.
Sole, Vicente A.
Srama, Ralf
Stephan, Thomas
Sterken, Veerle J.
Stodolna, Julien
Stroud, Rhonda M.
Sutton, Steven
Trieloff, Mario
Tsou, Peter
Tsuchiyama, Akira
Tyliszczak, Tolek
Vekemans, Bart
Vincze, Laszlo
Von Korff, Joshua
Wordsworth, Naomi
Zevin, Daniel
TI Stardust Interstellar Preliminary Examination II: Curating the
interstellar dust collector, picokeystones, and sources of impact tracks
SO METEORITICS & PLANETARY SCIENCE
LA English
DT Article
ID IRON-NICKEL SULFIDES; RADIATION PRESSURE; COMETARY DUST; AEROGEL;
PARTICLES; MISSION; FEATURES; GRAINS; DISKS; FOIL
AB We discuss the inherent difficulties that arise during "ground truth" characterization of the Stardust interstellar dust collector. The challenge of identifying contemporary interstellar dust impact tracks in aerogel is described within the context of background spacecraft secondaries and possible interplanetary dust particles and beta-meteoroids. In addition, the extraction of microscopic dust embedded in aerogel is technically challenging. Specifically, we provide a detailed description of the sample preparation techniques developed to address the unique goals and restrictions of the Interstellar Preliminary Exam. These sample preparation requirements and the scarcity of candidate interstellar impact tracks exacerbate the difficulties. We also illustrate the role of initial optical imaging with critically important examples, and summarize the overall processing of the collection to date.
C1 [Frank, David R.; Bastien, Ronald K.] NASA Johnson Space Ctr, ESCG, Houston, TX 77058 USA.
[Westphal, Andrew J.; Gainsforth, Zack; Butterworth, Anna L.; Anderson, David; Lettieri, Robert; Marchant, William; Stodolna, Julien; Von Korff, Joshua; Zevin, Daniel] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA USA.
[Zolensky, Michael E.; Allen, Carlton] NASA Johnson Space Ctr, ARES, Houston, TX USA.
[Ansari, Asna; Davis, Andrew M.; Heck, Philipp R.; Hvide, Brit] Field Museum Nat Hist, Robert A Pritzker Ctr Meteorit & Polar Studies, Chicago, IL 60605 USA.
[Bajt, Sasa] DESY, Hamburg, Germany.
[Bassim, Nabil; Stroud, Rhonda M.] Naval Res Lab, Mat Sci & Technol Div, Washington, DC USA.
[Bechtel, Hans A.; Tyliszczak, Tolek] Lawrence Berkeley Lab, Adv Light Source, Berkeley, CA USA.
[Borg, Janet] IAS Orsay, Orsay, France.
[Brenker, Frank E.; Schmitz, Sylvia] Goethe Univ Frankfurt, Inst Geosci, Frankfurt, Germany.
[Bridges, John] Univ Leicester, Space Res Ctr, Leicester, Leics, England.
[Brownlee, Donald E.] Univ Washington, Dept Astron, Seattle, WA 98195 USA.
[Burchell, Mark; Price, Mark C.] Univ Kent, Canterbury CT2 7NZ, Kent, England.
[Burghammer, Manfred; Cloetens, Peter; Tresseras, Juan-Angel Sans; Sole, Vicente A.] European Synchrotron Radiat Facil, F-38043 Grenoble, France.
[Changela, Hitesh] George Washington Univ, Washington, DC USA.
[Davis, Andrew M.; King, Ashley J.; Stephan, Thomas] Univ Chicago, Chicago, IL 60637 USA.
[Doll, Ryan; Floss, Christine; Leonard, Ariel; Ong, Wei Ja] Washington Univ, St Louis, MO USA.
[Flynn, George] SUNY Coll Plattsburgh, Plattsburgh, NY 12901 USA.
[Gruen, Eberhard; Sterken, Veerle J.] Max Planck Inst Kernphys, D-69117 Heidelberg, Germany.
[Hillier, Jon K.; Postberg, Frank; Trieloff, Mario] Heidelberg Univ, Inst Geowissensch, Heidelberg, Germany.
[Hoppe, Peter; Huth, Joachim; Leitner, Jan] Max Planck Inst Chem, D-55128 Mainz, Germany.
[Kearsley, Anton] Nat Hist Museum, London SW7 5BD, England.
[Lai, Barry; Sutton, Steven] Argonne Natl Lab, Adv Photon Source, Chicago, IL USA.
[Lemelle, Laurence] Ecole Normale Super Lyon, F-69364 Lyon, France.
[Leroux, Hugues] Univ Lille 1, Lille, France.
[Nittler, Larry R.] Carnegie Inst Sci, Washington, DC USA.
[Ogliore, Ryan] Univ Hawaii Manoa, Honolulu, HI 96822 USA.
[Sandford, Scott A.] NASA Ames Res Ctr, Moffett Field, CA USA.
[Schoonjans, Tom; Silversmit, Geert; Vekemans, Bart; Vincze, Laszlo] Univ Ghent, B-9000 Ghent, Belgium.
[Simionovici, Alexandre S.] Univ Grenoble, Observ Sci, Inst Sci Terre, Grenoble, France.
[Srama, Ralf] Univ Stuttgart, IRS, D-70174 Stuttgart, Germany.
[Sterken, Veerle J.] TU Braunschweig, IGEP, Braunschweig, Germany.
[Tsou, Peter] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Tsuchiyama, Akira] Osaka Univ, Osaka, Japan.
RP Frank, DR (reprint author), NASA Johnson Space Ctr, ESCG, Houston, TX 77058 USA.
EM david.r.frank@nasa.gov
RI Stroud, Rhonda/C-5503-2008; Sans Tresserras, Juan Angel/J-9362-2014;
Leitner, Jan/A-7391-2015; Hoppe, Peter/B-3032-2015; Bajt,
Sasa/G-2228-2010
OI Stroud, Rhonda/0000-0001-5242-8015; Burchell, Mark/0000-0002-2680-8943;
Sans Tresserras, Juan Angel/0000-0001-9047-3992; Leitner,
Jan/0000-0003-3655-6273; Hoppe, Peter/0000-0003-3681-050X;
FU NASA [NNX09AC36G, NNH11AQ61I]; Office of Science, Office of Basic Energy
Sciences, of the U.S. Department of Energy [DE-AC02-05CH11231]; U.S.
Department of Energy, Office of Science, Office of Basic Energy Sciences
[DE-AC02-98CH10886]
FX We thank P. Wozniekiewicz and C. Engrand for their thoughtful reviews
that greatly improved this manuscript. We also thank the AE John Bradley
for his critical input and time and effort spent reviewing the ISPE
manuscripts. The ISPE consortium gratefully acknowledges the NASA
Discovery Program for Stardust, the fourth NASA Discovery mission. We
are thankful for having the privilege of looking after the collection
and are gratefully indebted to the 30,000+ dusters who made this
possible. AJW, ALB, ZG, RL, DZ, WM and JVK were supported by NASA grant
NNX09AC36G. RMS, HCG and NDB were supported by NASA grant NNH11AQ61I.
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. Use of the National
Synchrotron Light Source, Brookhaven National Laboratory, was supported
by the U.S. Department of Energy, Office of Science, Office of Basic
Energy Sciences, under Contract No. DE-AC02-98CH10886.
NR 40
TC 13
Z9 13
U1 1
U2 18
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 1086-9379
EI 1945-5100
J9 METEORIT PLANET SCI
JI Meteorit. Planet. Sci.
PD SEP
PY 2014
VL 49
IS 9
SI SI
BP 1522
EP 1547
DI 10.1111/maps.12147
PG 26
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA AQ6HT
UT WOS:000342912100002
ER
PT J
AU Bechtel, HA
Flynn, GJ
Allen, C
Anderson, D
Ansari, A
Bajt, S
Bastien, RK
Bassim, N
Borg, J
Brenker, FE
Bridges, J
Brownlee, DE
Burchell, M
Burghammer, M
Butterworth, AL
Changela, H
Cloetens, P
Davis, AM
Doll, R
Floss, C
Frank, DR
Gainsforth, Z
Grun, E
Heck, PR
Hillier, JK
Hoppe, P
Hudson, B
Huth, J
Hvide, B
Kearsley, A
King, AJ
Lai, B
Leitner, J
Lemelle, L
Leroux, H
Leonard, A
Lettieri, R
Marchant, W
Nittler, LR
Ogliore, R
Ong, WJ
Postberg, F
Price, MC
Sandford, SA
Tresseras, JAS
Schmitz, S
Schoonjans, T
Silversmit, G
Simionovici, AS
Sole, VA
Srama, R
Stadermann, FJ
Stephan, T
Sterken, VJ
Stodolna, J
Stroud, RM
Sutton, S
Trieloff, M
Tsou, P
Tsuchiyama, A
Tyliszczak, T
Vekemans, B
Vincze, L
Von Korff, J
Westphal, AJ
Wordsworth, N
Zevin, D
Zolensky, ME
AF Bechtel, Hans A.
Flynn, George J.
Allen, Carlton
Anderson, David
Ansari, Asna
Bajt, Sasa
Bastien, Ron K.
Bassim, Nabil
Borg, Janet
Brenker, Frank E.
Bridges, John
Brownlee, Donald E.
Burchell, Mark
Burghammer, Manfred
Butterworth, Anna L.
Changela, Hitesh
Cloetens, Peter
Davis, Andrew M.
Doll, Ryan
Floss, Christine
Frank, David R.
Gainsforth, Zack
Gruen, Eberhard
Heck, Philipp R.
Hillier, Jon K.
Hoppe, Peter
Hudson, Bruce
Huth, Joachim
Hvide, Brit
Kearsley, Anton
King, Ashley J.
Lai, Barry
Leitner, Jan
Lemelle, Laurence
Leroux, Hugues
Leonard, Ariel
Lettieri, Robert
Marchant, William
Nittler, Larry R.
Ogliore, Ryan
Ong, Wei Ja
Postberg, Frank
Price, Mark C.
Sandford, Scott A.
Tresseras, Juan-Angel Sans
Schmitz, Sylvia
Schoonjans, Tom
Silversmit, Geert
Simionovici, Alexandre S.
Sole, Vicente A.
Srama, Ralf
Stadermann, Frank J.
Stephan, Thomas
Sterken, Veerle J.
Stodolna, Julien
Stroud, Rhonda M.
Sutton, Steven
Trieloff, Mario
Tsou, Peter
Tsuchiyama, Akira
Tyliszczak, Tolek
Vekemans, Bart
Vincze, Laszlo
Von Korff, Joshua
Westphal, Andrew J.
Wordsworth, Naomi
Zevin, Daniel
Zolensky, Michael E.
TI Stardust Interstellar Preliminary Examination III: Infrared
spectroscopic analysis of interstellar dust candidates
SO METEORITICS & PLANETARY SCIENCE
LA English
DT Article
ID COMET 81P/WILD 2; CONSTRAINTS; ORGANICS; RETURN; LIGHT
AB Under the auspices of the Stardust Interstellar Preliminary Examination, picokeystones extracted from the Stardust Interstellar Dust Collector were examined with synchrotron Fourier transform infrared (FTIR) microscopy to establish whether they contained extraterrestrial organic material. The picokeystones were found to be contaminated with varying concentrations and speciation of organics in the native aerogel, which hindered the search for organics in the interstellar dust candidates. Furthermore, examination of the picokeystones prior to and post X-ray microprobe analyses yielded evidence of beam damage in the form of organic deposition or modification, particularly with hard X-ray synchrotron X-ray fluorescence. From these results, it is clear that considerable care must be taken to interpret any organics that might be in interstellar dust particles. For the interstellar candidates examined thus far, however, there is no clear evidence of extraterrestrial organics associated with the track and/or terminal particles. However, we detected organic matter associated with the terminal particle in Track 37, likely a secondary impact from the Al-deck of the sample return capsule, demonstrating the ability of synchrotron FTIR to detect organic matter in small particles within picokeystones from the Stardust interstellar dust collector.
C1 [Bechtel, Hans A.; Tyliszczak, Tolek] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Adv Light Source, Berkeley, CA 94720 USA.
[Flynn, George J.] SUNY Coll Plattsburgh, Plattsburgh, NY 12901 USA.
[Allen, Carlton; Zolensky, Michael E.] NASA Johnson Space Ctr, ARES, Houston, TX USA.
[Anderson, David; Butterworth, Anna L.; Gainsforth, Zack; Lettieri, Robert; Marchant, William; Stodolna, Julien; Von Korff, Joshua; Westphal, Andrew J.; Zevin, Daniel] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA USA.
[Ansari, Asna; Heck, Philipp R.; Hvide, Brit; King, Ashley J.] Field Museum Nat Hist, Robert A Pritzker Ctr Meteorit & Polar Studies, Chicago, IL 60605 USA.
[Bajt, Sasa] DESY, Hamburg, Germany.
[Bastien, Ron K.; Frank, David R.] NASA Johnson Space Ctr, ESCG, Houston, TX USA.
[Bassim, Nabil; Stroud, Rhonda M.] Naval Res Lab, Mat Sci & Technol Div, Washington, DC USA.
[Borg, Janet] IAS Orsay, Orsay, France.
[Brenker, Frank E.; Schmitz, Sylvia] Goethe Univ Frankfurt, Inst Geosci, Frankfurt, Germany.
[Bridges, John] Univ Leicester, Space Res Ctr, Leicester, Leics, England.
[Brownlee, Donald E.] Univ Washington, Dept Astron, Seattle, WA 98195 USA.
[Burchell, Mark; Price, Mark C.] Univ Kent, Canterbury, Kent, England.
[Burghammer, Manfred; Cloetens, Peter; Tresseras, Juan-Angel Sans; Sole, Vicente A.] European Synchrotron Radiat Facil, F-38043 Grenoble, France.
[Changela, Hitesh] George Washington Univ, Washington, DC USA.
[Davis, Andrew M.; King, Ashley J.; Stephan, Thomas] Univ Chicago, Chicago, IL 60637 USA.
[Doll, Ryan; Floss, Christine; Leonard, Ariel; Ong, Wei Ja; Stadermann, Frank J.] Washington Univ, St Louis, MO USA.
[Gruen, Eberhard; Sterken, Veerle J.] Max Planck Inst Kernphys, D-69117 Heidelberg, Germany.
[Hillier, Jon K.; Postberg, Frank; Trieloff, Mario] Heidelberg Univ, Inst Geowissensch, Heidelberg, Germany.
[Hoppe, Peter; Huth, Joachim; Leitner, Jan] Max Planck Inst Chem, D-55128 Mainz, Germany.
[Kearsley, Anton] Nat Hist Museum, London SW7 5BD, England.
[Lai, Barry; Sutton, Steven] Argonne Natl Lab, Adv Photon Source, Chicago, IL USA.
[Lemelle, Laurence] Ecole Normale Super Lyon, F-69364 Lyon, France.
[Leroux, Hugues] Univ Lille 1, Lille 1, France.
[Nittler, Larry R.] Carnegie Inst Sci, Washington, DC USA.
[Ogliore, Ryan] Univ Hawaii Manoa, Honolulu, HI 96822 USA.
[Postberg, Frank; Srama, Ralf; Sterken, Veerle J.] Univ Stuttgart, Inst Raumfahrtsyst, Stuttgart, Germany.
[Sandford, Scott A.] NASA Ames Res Ctr, Moffett Field, CA USA.
[Schoonjans, Tom; Silversmit, Geert; Vekemans, Bart; Vincze, Laszlo] Univ Ghent, B-9000 Ghent, Belgium.
[Simionovici, Alexandre S.] Univ Grenoble, Observ Sci, Inst Sci Terre, Grenoble, France.
[Sterken, Veerle J.] TU Braunschweig, Inst Geophys & Extraterrestr Phys, Braunschweig, Germany.
[Tsou, Peter] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Tsuchiyama, Akira] Osaka Univ, Osaka, Japan.
RP Bechtel, HA (reprint author), Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Adv Light Source, Berkeley, CA 94720 USA.
EM habechtel@lbl.gov
RI Sans Tresserras, Juan Angel/J-9362-2014; Leitner, Jan/A-7391-2015;
Hoppe, Peter/B-3032-2015; Bajt, Sasa/G-2228-2010; Stroud,
Rhonda/C-5503-2008;
OI Sans Tresserras, Juan Angel/0000-0001-9047-3992; Leitner,
Jan/0000-0003-3655-6273; Hoppe, Peter/0000-0003-3681-050X; Stroud,
Rhonda/0000-0001-5242-8015; Burchell, Mark/0000-0002-2680-8943
FU NASA Laboratory Analysis of Returned Samples research grant
[NNX11AE15G]; NASA [NNX09AC36G, NNH11AQ61I]; Office of Science, Office
of Basic Energy Sciences, of the U.S. Department of Energy
[DE-AC02-05CH11231]; U.S. Department of Energy, Office of Science,
Office of Basic Energy Sciences [DE-AC02-98CH10886]
FX The ISPE consortium gratefully acknowledges the NASA Discovery Program
for Stardust, the fourth NASA Discovery mission. GJF was supported by a
NASA Laboratory Analysis of Returned Samples research grant NNX11AE15G.
AJW, ALB, ZG, RL, DZ, WM, and JVK were supported by NASA grant
NNX09AC36G. RMS, HCG, and NDB were supported by NASA grant NNH11AQ61I.
The ALS 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. Use of the NSLS, BNL, was supported by the U.S.
Department of Energy, Office of Science, Office of Basic Energy
Sciences, under Contract No. DE-AC02-98CH10886.
NR 30
TC 6
Z9 6
U1 2
U2 14
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 1086-9379
EI 1945-5100
J9 METEORIT PLANET SCI
JI Meteorit. Planet. Sci.
PD SEP
PY 2014
VL 49
IS 9
SI SI
BP 1548
EP 1561
DI 10.1111/maps.12125
PG 14
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA AQ6HT
UT WOS:000342912100003
ER
PT J
AU Butterworth, AL
Westphal, AJ
Tyliszczak, T
Gainsforth, Z
Stodolna, J
Frank, DR
Allen, C
Anderson, D
Ansari, A
Bajt, S
Bastien, RK
Bassim, N
Bechtel, HA
Borg, J
Brenker, FE
Bridges, J
Brownlee, DE
Burchell, M
Burghammer, M
Changela, H
Cloetens, P
Davis, AM
Doll, R
Floss, C
Flynn, G
Grun, E
Heck, PR
Hillier, JK
Hoppe, P
Hudson, B
Huth, J
Hvide, B
Kearsley, A
King, AJ
Lai, B
Leitner, J
Lemelle, L
Leroux, H
Leonard, A
Lettieri, R
Marchant, W
Nittler, LR
Ogliore, R
Ong, WJ
Postberg, F
Price, MC
Sandford, SA
Tresseras, JAS
Schmitz, S
Schoonjans, T
Silversmit, G
Simionovici, AS
Sole, VA
Srama, R
Stadermann, FJ
Stephan, T
Sterken, VJ
Stroud, RM
Sutton, S
Trieloff, M
Tsou, P
Tsuchiyama, A
Vekemans, B
Vincze, L
Von Korff, J
Wordsworth, N
Zevin, D
Zolensky, ME
AF Butterworth, Anna L.
Westphal, Andrew J.
Tyliszczak, Tolek
Gainsforth, Zack
Stodolna, Julien
Frank, David R.
Allen, Carlton
Anderson, David
Ansari, Asna
Bajt, Sasa
Bastien, Ron K.
Bassim, Nabil
Bechtel, Hans A.
Borg, Janet
Brenker, Frank E.
Bridges, John
Brownlee, Donald E.
Burchell, Mark
Burghammer, Manfred
Changela, Hitesh
Cloetens, Peter
Davis, Andrew M.
Doll, Ryan
Floss, Christine
Flynn, George
Gruen, Eberhard
Heck, Philipp R.
Hillier, Jon K.
Hoppe, Peter
Hudson, Bruce
Huth, Joachim
Hvide, Brit
Kearsley, Anton
King, Ashley J.
Lai, Barry
Leitner, Jan
Lemelle, Laurence
Leroux, Hugues
Leonard, Ariel
Lettieri, Robert
Marchant, William
Nittler, Larry R.
Ogliore, Ryan
Ong, Wei Ja
Postberg, Frank
Price, Mark C.
Sandford, Scott A.
Tresseras, Juan-Angel Sans
Schmitz, Sylvia
Schoonjans, Tom
Silversmit, Geert
Simionovici, Alexandre S.
Sole, Vicente A.
Srama, Ralf
Stadermann, Frank J.
Stephan, Thomas
Sterken, Veerle J.
Stroud, Rhonda M.
Sutton, Steven
Trieloff, Mario
Tsou, Peter
Tsuchiyama, Akira
Vekemans, Bart
Vincze, Laszlo
Von Korff, Joshua
Wordsworth, Naomi
Zevin, Daniel
Zolensky, Michael E.
TI Stardust Interstellar Preliminary Examination IV: Scanning transmission
X-ray microscopy analyses of impact features in the Stardust
Interstellar Dust Collector
SO METEORITICS & PLANETARY SCIENCE
LA English
DT Article
ID NEAR-EDGE STRUCTURE; K-EDGE; ABSORPTION SPECTROSCOPY; MINERALS; AL;
XANES; TEMPERATURE; MAGNESIUM; RANGE; MG
AB We report the quantitative characterization by synchrotron soft X-ray spectroscopy of 31 potential impact features in the aerogel capture medium of the Stardust Interstellar Dust Collector. Samples were analyzed in aerogel by acquiring high spatial resolution maps and high energy-resolution spectra of major rock-forming elements Mg, Al, Si, Fe, and others. We developed diagnostic screening tests to reject spacecraft secondary ejecta and terrestrial contaminants from further consideration as interstellar dust candidates. The results support an extraterrestrial origin for three interstellar candidates: I1043,1,30 (Orion) is a 3 pg particle with Mg-spinel, forsterite, and an iron-bearing phase. I1047,1,34 (Hylabrook) is a 4 pg particle comprising an olivine core surrounded by low-density, amorphous Mg-silicate and amorphous Fe, Cr, and Mn phases. I1003,1,40 (Sorok) has the track morphology of a high-speed impact, but contains no detectable residue that is convincingly distinguishable from the background aerogel. Twenty-two samples with an anthropogenic origin were rejected, including four secondary ejecta from impacts on the Stardust spacecraft aft solar panels, nine ejecta from secondary impacts on the Stardust Sample Return Capsule, and nine contaminants lacking evidence of an impact. Other samples in the collection included I1029,1,6, which contained surviving solar system impactor material. Four samples remained ambiguous: I1006,2,18, I1044,2,32, and I1092,2,38 were too dense for analysis, and we did not detect an intact projectile in I1044,3,33. We detected no radiation effects from the synchrotron soft X-ray analyses; however, we recorded the effects of synchrotron hard X-ray radiation on I1043,1,30 and I1047,1,34.
C1 [Butterworth, Anna L.; Westphal, Andrew J.; Gainsforth, Zack; Stodolna, Julien; Anderson, David; Lettieri, Robert; Marchant, William; Von Korff, Joshua; Zevin, Daniel] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
[Tyliszczak, Tolek; Bechtel, Hans A.] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Adv Light Source, Berkeley, CA 94720 USA.
[Frank, David R.; Bastien, Ron K.] NASA JSC, ESCG, Houston, TX USA.
[Allen, Carlton; Zolensky, Michael E.] NASA JSC, ARES, Houston, TX USA.
[Ansari, Asna; Heck, Philipp R.; Hvide, Brit] Field Museum Nat Hist, Robert A Pritzker Ctr Meteorit & Polar Studies, Chicago, IL 60605 USA.
[Bajt, Sasa] DESY, Hamburg, Germany.
[Bassim, Nabil; Stroud, Rhonda M.] Naval Res Lab, Mat Sci & Technol Div, Washington, DC USA.
[Borg, Janet] Inst Astrophys Spatiale, Orsay, France.
[Brenker, Frank E.; Schmitz, Sylvia] Goethe Univ Frankfurt, Inst Geosci, Frankfurt, Germany.
[Bridges, John] Univ Leicester, Space Res Ctr, Leicester, Leics, England.
[Brownlee, Donald E.] Univ Washington, Dept Astron, Seattle, WA 98195 USA.
[Burchell, Mark; Price, Mark C.] Univ Kent, Canterbury, Kent, England.
[Burghammer, Manfred; Cloetens, Peter; Tresseras, Juan-Angel Sans; Sole, Vicente A.] European Synchrotron Radiat Facil, F-38043 Grenoble, France.
[Changela, Hitesh] George Washington Univ, Washington, DC USA.
[Davis, Andrew M.; King, Ashley J.; Stephan, Thomas] Univ Chicago, Dept Geophys Sci, Chicago, IL 60637 USA.
[Doll, Ryan; Floss, Christine; Leonard, Ariel; Ong, Wei Ja; Stadermann, Frank J.] Washington Univ, Dept Phys, St Louis, MO 63130 USA.
[Flynn, George] SUNY Coll Plattsburgh, Dept Phys, Plattsburgh, NY 12901 USA.
[Gruen, Eberhard; Sterken, Veerle J.] Max Planck Inst Kernphys, D-69117 Heidelberg, Germany.
[Hillier, Jon K.; Postberg, Frank; Trieloff, Mario] Heidelberg Univ, Inst Geowissensch, Heidelberg, Germany.
[Hoppe, Peter; Huth, Joachim; Leitner, Jan] Max Planck Inst Chem, D-55128 Mainz, Germany.
[Kearsley, Anton] Nat Hist Museum, London SW7 5BD, England.
[Lai, Barry; Sutton, Steven] Argonne Natl Lab, Adv Photon Source, Chicago, IL USA.
[Lemelle, Laurence] Ecole Normale Super Lyon, F-69364 Lyon, France.
[Leroux, Hugues] Univ Lille, Lille, France.
[Nittler, Larry R.] Carnegie Inst Sci, Washington, DC USA.
[Ogliore, Ryan] Univ Hawaii Manoa, Honolulu, HI 96822 USA.
[Sandford, Scott A.] NASA Ames Res Ctr, Moffett Field, CA USA.
[Schoonjans, Tom; Silversmit, Geert; Vekemans, Bart; Vincze, Laszlo] Univ Ghent, B-9000 Ghent, Belgium.
[Simionovici, Alexandre S.] Univ Grenoble, Observ Sci, Inst Sci Terre, Grenoble, France.
[Srama, Ralf; Sterken, Veerle J.] Univ Stuttgart, Inst Raumfahrtsyst, D-70174 Stuttgart, Germany.
[Sterken, Veerle J.] Tech Univ Carolo Wilhelmina Braunschweig, Inst Geophys & Extraterrestr Phys, D-38106 Braunschweig, Germany.
[Tsou, Peter] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Tsuchiyama, Akira] Osaka Univ, Osaka, Japan.
RP Butterworth, AL (reprint author), Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
EM annab@ssl.berkeley.edu
RI Bajt, Sasa/G-2228-2010; Stroud, Rhonda/C-5503-2008; Sans Tresserras,
Juan Angel/J-9362-2014; Leitner, Jan/A-7391-2015; Hoppe,
Peter/B-3032-2015
OI Stroud, Rhonda/0000-0001-5242-8015; Burchell, Mark/0000-0002-2680-8943;
Sans Tresserras, Juan Angel/0000-0001-9047-3992; Leitner,
Jan/0000-0003-3655-6273; Hoppe, Peter/0000-0003-3681-050X
FU NASA [NNX09AC36G, NNH11AQ61I]; Office of Science, Office of Basic Energy
Sciences, of the U.S. Department of Energy [DE-AC02-05CH11231]; U.S.
Department of Energy, Office of Science, Office of Basic Energy Sciences
[DE-AC02-98CH10886]
FX The ISPE consortium gratefully acknowledges the NASA Discovery Program
for Stardust, the fourth NASA Discovery mission. AJW, ALB, ZG, RL, DZ,
WM, and JVK were supported by NASA grant NNX09AC36G. RMS, HCG, and NDB
were supported by NASA grant NNH11AQ61I. The ALS 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. Use of
the National Synchrotron Light Source, Brookhaven National Laboratory,
was supported by the U.S. Department of Energy, Office of Science,
Office of Basic Energy Sciences, under Contract No. DE-AC02-98CH10886.
We appreciate greatly the thorough reviews by one anonymous reviewer,
John Bradley, and associate editor, Christian Koeberl. Their
contributions improved the manuscript and helped to clarify key
findings. We thank Steve Boggs for helpful discussions regarding X-ray
dose estimates in the Interstellar Medium, and for providing diffuse
X-ray data. We thank the Natural History Museum, London, for providing
most of the standards used for acquiring the XANES spectra library in
this work.
NR 33
TC 12
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U1 0
U2 15
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 1086-9379
EI 1945-5100
J9 METEORIT PLANET SCI
JI Meteorit. Planet. Sci.
PD SEP
PY 2014
VL 49
IS 9
SI SI
BP 1562
EP 1593
DI 10.1111/maps.12220
PG 32
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA AQ6HT
UT WOS:000342912100004
ER
PT J
AU Brenker, FE
Westphal, AJ
Vincze, L
Burghammer, M
Schmitz, S
Schoonjans, T
Silversmit, G
Vekemans, B
Allen, C
Anderson, D
Ansari, A
Bajt, S
Bastien, RK
Bassim, N
Bechtel, HA
Borg, J
Bridges, J
Brownlee, DE
Burchell, M
Butterworth, AL
Changela, H
Cloetens, P
Davis, AM
Doll, R
Floss, C
Flynn, G
Fougeray, P
Frank, DR
Gainsforth, Z
Grun, E
Heck, PR
Hillier, JK
Hoppe, P
Hudson, B
Huth, J
Hvide, B
Kearsley, A
King, AJ
Lai, B
Leitner, J
Lemelle, L
Leroux, H
Leonard, A
Lettieri, R
Marchant, W
Nittler, LR
Ogliore, R
Ong, WJ
Postberg, F
Price, MC
Sandford, SA
Tresseras, JAS
Simionovici, AS
Sole, VA
Srama, R
Stadermann, F
Stephan, T
Sterken, VJ
Stodolna, J
Stroud, RM
Sutton, S
Trieloff, M
Tsou, P
Tsuchiyama, A
Tyliszczak, T
Von Korff, J
Wordsworth, N
Zevin, D
Zolensky, ME
AF Brenker, Frank E.
Westphal, Andrew J.
Vincze, Laszlo
Burghammer, Manfred
Schmitz, Sylvia
Schoonjans, Tom
Silversmit, Geert
Vekemans, Bart
Allen, Carlton
Anderson, David
Ansari, Asna
Bajt, Sasa
Bastien, Ron K.
Bassim, Nabil
Bechtel, Hans A.
Borg, Janet
Bridges, John
Brownlee, Donald E.
Burchell, Mark
Butterworth, Anna L.
Changela, Hitesh
Cloetens, Peter
Davis, Andrew M.
Doll, Ryan
Floss, Christine
Flynn, George
Fougeray, Patrick
Frank, David R.
Gainsforth, Zack
Gruen, Eberhard
Heck, Philipp R.
Hillier, Jon K.
Hoppe, Peter
Hudson, Bruce
Huth, Joachim
Hvide, Brit
Kearsley, Anton
King, Ashley J.
Lai, Barry
Leitner, Jan
Lemelle, Laurence
Leroux, Hugues
Leonard, Ariel
Lettieri, Robert
Marchant, William
Nittler, Larry R.
Ogliore, Ryan
Ong, Wei Ja
Postberg, Frank
Price, Mark C.
Sandford, Scott A.
Tresseras, Juan-Angel Sans
Simionovici, Alexandre S.
Sole, Vicente A.
Srama, Ralf
Stadermann, Frank
Stephan, Thomas
Sterken, Veerle J.
Stodolna, Julien
Stroud, Rhonda M.
Sutton, Steven
Trieloff, Mario
Tsou, Peter
Tsuchiyama, Akira
Tyliszczak, Tolek
Von Korff, Joshua
Wordsworth, Naomi
Zevin, Daniel
Zolensky, Michael E.
TI Stardust Interstellar Preliminary Examination V: XRF analyses of
interstellar dust candidates at ESRF ID13
SO METEORITICS & PLANETARY SCIENCE
LA English
DT Article
ID INTERPLANETARY DUST; AEROGEL; OLIVINE
AB Here, we report analyses by synchrotron X-ray fluorescence microscopy of the elemental composition of eight candidate impact features extracted from the Stardust Interstellar Dust Collector (SIDC). Six of the features were unambiguous tracks, and two were crater-like features. Five of the tracks are so-called "midnight" tracks-that is, they had trajectories consistent with an origin either in the interstellar dust stream or as secondaries from impacts on the Sample Return Capsule (SRC). In a companion paper reporting synchrotron X-ray diffraction analyses of ISPE candidates, we show that two of these particles contain natural crystalline materials: the terminal particle of track 30 contains olivine and spinel, and the terminal particle of track 34 contains olivine. Here, we show that the terminal particle of track 30, Orion, shows elemental abundances, normalized to Fe, that are close to CI values, and a complex, fine-grained structure. The terminal particle of track 34, Hylabrook, shows abundances that deviate strongly from CI, but shows little fine structure and is nearly homogenous. The terminal particles of other midnight tracks, 29 and 37, had heavy element abundances below detection threshold. A third, track 28, showed a composition inconsistent with an extraterrestrial origin, but also inconsistent with known spacecraft materials. A sixth track, with a trajectory consistent with secondary ejecta from an impact on one of the spacecraft solar panels, contains abundant Ce and Zn. This is consistent with the known composition of the glass covering the solar panel. Neither crater-like feature is likely to be associated with extraterrestrial materials. We also analyzed blank aerogel samples to characterize background and variability between aerogel tiles. We found significant differences in contamination levels and compositions, emphasizing the need for local background subtraction for accurate quantification.
C1 [Brenker, Frank E.; Schmitz, Sylvia] Goethe Univ Frankfurt, D-60438 Frankfurt, Germany.
[Westphal, Andrew J.; Anderson, David; Butterworth, Anna L.; Gainsforth, Zack; Lettieri, Robert; Marchant, William; Stodolna, Julien; Von Korff, Joshua; Zevin, Daniel] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
[Vincze, Laszlo; Schoonjans, Tom; Silversmit, Geert; Vekemans, Bart] Univ Ghent, Dept Analyt Chem, B-9000 Ghent, Belgium.
[Burghammer, Manfred; Cloetens, Peter; Tresseras, Juan-Angel Sans; Sole, Vicente A.] European Synchrotron Radiat Facil, F-38043 Grenoble, France.
[Ansari, Asna; Hvide, Brit; King, Ashley J.] Field Museum Nat Hist, Robert A Pritzker Ctr Meteorit & Polar Studies, Chicago, IL 60605 USA.
[Bajt, Sasa] DESY, D-22607 Hamburg, Germany.
[Bastien, Ron K.; Frank, David R.] NASA, Lyndon B Johnson Space Ctr, ESCG, Houston, TX 77058 USA.
[Bassim, Nabil; Stroud, Rhonda M.] Naval Res Lab, Nanoscale Mat Sect, Washington, DC 20375 USA.
[Bechtel, Hans A.; Tyliszczak, Tolek] Lawrence Berkeley Lab, Adv Light Source, Berkeley, CA 94720 USA.
[Borg, Janet] IAS Orsay, Orsay, France.
[Bridges, John] Univ Leicester, Space Res Ctr, Dept Phys & Astron, Leicester LE1 7RH, Leics, England.
[Brownlee, Donald E.] Univ Washington, Dept Astron, Seattle, WA 98195 USA.
[Burchell, Mark; Price, Mark C.] Univ Kent, Canterbury CT2 7NR, Kent, England.
[Changela, Hitesh] George Washington Univ, Washington, DC 20052 USA.
[Davis, Andrew M.; Stephan, Thomas] Univ Chicago, Chicago, IL 60637 USA.
[Doll, Ryan; Floss, Christine; Leonard, Ariel; Ong, Wei Ja; Stadermann, Frank] Washington Univ, St Louis, MO 63130 USA.
[Flynn, George] SUNY Coll Plattsburgh, Dept Phys, Plattsburgh, NY 12901 USA.
[Fougeray, Patrick] Chigy, Burgundy, Chigy, France.
[Gruen, Eberhard] Max Planck Inst Kernphys, D-69117 Heidelberg, Germany.
[Heck, Philipp R.; Hillier, Jon K.; Postberg, Frank] Inst Geowissensch, D-69120 Heidelberg, Germany.
[Hoppe, Peter; Huth, Joachim; Leitner, Jan] Max Planck Inst Chem, D-55128 Mainz, Germany.
[Kearsley, Anton] Nat Hist Museum, London SW7 5BD, England.
[Lai, Barry; Sutton, Steven] Argonne Natl Lab, Adv Photon Source, Argonne, IL 60439 USA.
[Lemelle, Laurence] Ecole Normale Super Lyon, F-69364 Lyon, France.
[Leroux, Hugues] Univ Lille 1, Unite Mat & Transformat UMR 8207, F-59655 Villeneuve Dascq, France.
[Nittler, Larry R.] Carnegie Inst Sci, Dept Terr Magnetism, Washington, DC 20015 USA.
[Ogliore, Ryan] Univ Hawaii Manoa, Sch Ocean & Earth Sci & Technol, Hawaii Inst Geophys & Planetary Sci, Honolulu, HI 96822 USA.
[Sandford, Scott A.] NASA, Ames Res Ctr, Astrophys Branch, Moffett Field, CA 94035 USA.
[Simionovici, Alexandre S.] Univ Grenoble, Observ Sci, Inst Sci Terre, Grenoble, France.
[Srama, Ralf; Sterken, Veerle J.] Univ Stuttgart, Inst Raumfahrtsyst, D-70569 Stuttgart, Germany.
[Trieloff, Mario] Inst Geowissensch, D-69120 Heidelberg, Germany.
[Tsou, Peter] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Tsuchiyama, Akira] Osaka Univ, Grad Sch Sci, Dept Earth & Planetary Sci, Osaka, Japan.
RP Westphal, AJ (reprint author), Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
EM westphal@ssl.berkeley.edu
RI Bajt, Sasa/G-2228-2010; Stroud, Rhonda/C-5503-2008; Sans Tresserras,
Juan Angel/J-9362-2014; Leitner, Jan/A-7391-2015; Hoppe,
Peter/B-3032-2015
OI Stroud, Rhonda/0000-0001-5242-8015; Burchell, Mark/0000-0002-2680-8943;
Sans Tresserras, Juan Angel/0000-0001-9047-3992; Leitner,
Jan/0000-0003-3655-6273; Hoppe, Peter/0000-0003-3681-050X
FU NASA [NNX09AC36G, NNH11AQ61I]; Office of Science, Office of Basic Energy
Sciences, of the U.S. Department of Energy [DE-AC02-05CH11231]; U.S.
Department of Energy, Office of Science, Office of Basic Energy Sciences
[DE-AC02-98CH10886]; German Science Foundation (DFG)
FX This manuscript was improved due to the thoughtful comments of John
Bradley. The ISPE consortium gratefully acknowledge the NASA Discovery
Program for Stardust, the fourth NASA Discovery mission. AJW, ALB, ZG,
RL, DZ, WM, and JVK were supported by NASA grant NNX09AC36G. We thank
Steve Boggs for astrophysical soft X-ray spectra. RMS, HCG, and NDB were
supported by NASA grant NNH11AQ61I. 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. Use of the National Synchrotron Light Source,
Brookhaven National Laboratory, was supported by the U.S. Department of
Energy, Office of Science, Office of Basic Energy Sciences, under
Contract no. DE-AC02-98CH10886. We like to thank the ESRF for the
allocated beamtime at ID13, instrumental and technical support. FEB and
SS were supported by funding of the German Science Foundation (DFG).
NR 28
TC 9
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U1 1
U2 16
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 1086-9379
EI 1945-5100
J9 METEORIT PLANET SCI
JI Meteorit. Planet. Sci.
PD SEP
PY 2014
VL 49
IS 9
SI SI
BP 1594
EP 1611
DI 10.1111/maps.12206
PG 18
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA AQ6HT
UT WOS:000342912100005
ER
PT J
AU Simionovici, AS
Lemelle, L
Cloetens, P
Sole, VA
Tresseras, JAS
Butterworth, AL
Westphal, AJ
Gainsforth, Z
Stodolna, J
Allen, C
Anderson, D
Ansari, A
Bajt, S
Bassim, N
Bastien, RK
Bechtel, HA
Borg, J
Brenker, FE
Bridges, J
Brownlee, DE
Burchell, M
Burghammer, M
Changela, H
Davis, AM
Doll, R
Floss, C
Flynn, G
Frank, DR
Grun, E
Heck, PR
Hillier, JK
Hoppe, P
Hudson, B
Huth, J
Hvide, B
Kearsley, A
King, AJ
Lai, B
Leitner, J
Leonard, A
Leroux, H
Lettieri, R
Marchant, W
Nittler, LR
Ogliore, R
Ong, WJ
Postberg, F
Price, MC
Sandford, SA
Schmitz, S
Schoonjans, T
Silversmit, G
Srama, R
Stadermann, FJ
Stephan, T
Sterken, VJ
Stroud, RM
Sutton, S
Trieloff, M
Tsou, P
Tsuchiyama, A
Tyliszczak, T
Vekemans, B
Vincze, L
Von Korff, J
Wordsworth, N
Zevin, D
Zolensky, ME
AF Simionovici, Alexandre S.
Lemelle, Laurence
Cloetens, Peter
Sole, Vicente A.
Tresseras, Juan-Angel Sans
Butterworth, Anna L.
Westphal, Andrew J.
Gainsforth, Zack
Stodolna, Julien
Allen, Carlton
Anderson, David
Ansari, Asna
Bajt, Sasa
Bassim, Nabil
Bastien, Ron K.
Bechtel, Hans A.
Borg, Janet
Brenker, Frank E.
Bridges, John
Brownlee, Donald E.
Burchell, Mark
Burghammer, Manfred
Changela, Hitesh
Davis, Andrew M.
Doll, Ryan
Floss, Christine
Flynn, George
Frank, David R.
Gruen, Eberhard
Heck, Philipp R.
Hillier, Jon K.
Hoppe, Peter
Hudson, Bruce
Huth, Joachim
Hvide, Brit
Kearsley, Anton
King, Ashley J.
Lai, Barry
Leitner, Jan
Leonard, Ariel
Leroux, Hugues
Lettieri, Robert
Marchant, William
Nittler, Larry R.
Ogliore, Ryan
Ong, Wei Ja
Postberg, Frank
Price, Mark C.
Sandford, Scott A.
Schmitz, Sylvia
Schoonjans, Tom
Silversmit, Geert
Srama, Ralf
Stadermann, Frank J.
Stephan, Thomas
Sterken, Veerle J.
Stroud, Rhonda M.
Sutton, Steven
Trieloff, Mario
Tsou, Peter
Tsuchiyama, Akira
Tyliszczak, Tolek
Vekemans, Bart
Vincze, Laszlo
Von Korff, Joshua
Wordsworth, Naomi
Zevin, Daniel
Zolensky, Michael E.
TI Stardust Interstellar Preliminary Examination VI: Quantitative elemental
analysis by synchrotron X-ray fluorescence nanoimaging of eight impact
features in aerogel
SO METEORITICS & PLANETARY SCIENCE
LA English
DT Article
ID COMET 81P/WILD-2; SOLAR-SYSTEM; DUST; GRAINS; CLOUD; GAS
AB Hard X-ray, quantitative, fluorescence elemental imaging was performed on the ID22NI nanoprobe and ID22 microprobe beam lines of the European Synchrotron Research facility (ESRF) in Grenoble, France, on eight interstellar candidate impact features in the framework of the NASA Stardust Interstellar Preliminary Examination (ISPE). Three features were unambiguous tracks, and the other five were identified as possible, but not definite, impact features. Overall, we produced an absolute quantification of elemental abundances in the 15 <= Z <= 30 range by means of corrections of the beam parameters, reference materials, and fundamental atomic parameters. Seven features were ruled out as interstellar dust candidates (ISDC) based on compositional arguments. One of the three tracks, I1043,1,30,0,0, contained, at the time of our analysis, two physically separated, micrometer-sized terminal particles, the most promising ISDCs, Orion and Sirius. We found that the Sirius particle was a fairly homogenous Ni-bearing particle and contained about 33 fg of distributed high-Z elements (Z > 12). Orion was a highly heterogeneous Fe-bearing particle and contained about 59 fg of heavy elements located in hundred nanometer phases, forming an irregular mantle that surrounded a low-Z core. X-ray diffraction (XRD) measurements revealed Sirius to be amorphous, whereas Orion contained partially crystalline material (Gainsforth et al. 2014). Within the mantle, one grain was relatively Fe-Ni-Mn-rich; other zones were relatively Mn-Cr-Ti-rich and may correspond to different spinel populations. For absolute quantification purposes, Orion was assigned to a mineralogical assemblage of forsterite, spinel, and an unknown Fe-bearing phase, while Sirius was most likely composed of an amorphous Mg-bearing material with minor Ni and Fe. Owing to its nearly chondritic abundances of the nonvolatile elements Ca, Ti, Co, and Ni with respect to Fe, in combination with the presence of olivine and spinel as inferred from XRD measurements, Orion had a high probability of being extraterrestrial in origin.
C1 [Simionovici, Alexandre S.] Univ Grenoble, Observ Sci, Inst Sci Terre, Grenoble, France.
[Lemelle, Laurence] Ecole Normale Super Lyon, CNRS, LGL LJC, F-69364 Lyon, France.
[Cloetens, Peter; Sole, Vicente A.; Tresseras, Juan-Angel Sans; Burghammer, Manfred] European Synchrotron Radiat Facil, F-38043 Grenoble, France.
[Butterworth, Anna L.; Westphal, Andrew J.; Gainsforth, Zack; Stodolna, Julien; Anderson, David; Lettieri, Robert; Marchant, William; Von Korff, Joshua; Zevin, Daniel] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA USA.
[Allen, Carlton; Bastien, Ron K.; Frank, David R.; Zolensky, Michael E.] NASA JSC, ESCG, Houston, TX USA.
[Ansari, Asna; Heck, Philipp R.; Hvide, Brit] Field Museum Nat Hist, Robert A Pritzker Ctr Meteorit & Polar Studies, Chicago, IL 60605 USA.
[Bajt, Sasa] DESY, Hamburg, Germany.
[Bassim, Nabil] Naval Res Lab, Washington, DC USA.
[Bechtel, Hans A.; Tyliszczak, Tolek] Lawrence Berkeley Lab, Adv Light Source, Berkeley, CA USA.
[Brenker, Frank E.; Schmitz, Sylvia] Goethe Univ Frankfurt, Inst Geosci, Frankfurt, Germany.
[Bridges, John] Univ Leicester, Space Res Ctr, Leicester, Leics, England.
[Brownlee, Donald E.] Univ Washington, Dept Astron, Seattle, WA 98195 USA.
[Burchell, Mark; Price, Mark C.] Univ Kent, Sch Phys Sci, Canterbury, Kent, England.
[Changela, Hitesh] George Washington Univ, Dept Phys, Washington, DC 20052 USA.
[Davis, Andrew M.; King, Ashley J.; Stephan, Thomas] Univ Chicago, Dept Geophys Sci, Chicago, IL 60637 USA.
[Doll, Ryan; Floss, Christine; Leonard, Ariel; Ong, Wei Ja; Stadermann, Frank J.] Washington Univ, Dept Phys, St Louis, MO 63130 USA.
[Flynn, George] SUNY Coll Plattsburgh, Plattsburgh, NY 12901 USA.
[Gruen, Eberhard; Leitner, Jan] Max Planck Inst Kernphys, D-69117 Heidelberg, Germany.
[Hillier, Jon K.; Postberg, Frank; Trieloff, Mario] Heidelberg Univ, Inst Geowissensch, Heidelberg, Germany.
[Hoppe, Peter; Huth, Joachim; Sterken, Veerle J.] Max Planck Inst Chem, D-55128 Mainz, Germany.
[Kearsley, Anton] Nat Hist Museum, London SW7 5BD, England.
[Lai, Barry; Sutton, Steven] Argonne Natl Lab, Adv Photon Source, Chicago, IL USA.
[Leroux, Hugues] Univ Lille 1, F-59655 Villeneuve Dascq, France.
[Nittler, Larry R.] Carnegie Inst Sci, Washington, DC USA.
[Ogliore, Ryan] Univ Hawaii Manoa, Inst Geophys & Planetol, Honolulu, HI 96822 USA.
[Sandford, Scott A.] NASA Ames Res Ctr, Moffett Field, CA USA.
[Schoonjans, Tom; Silversmit, Geert; Vekemans, Bart; Vincze, Laszlo] Univ Ghent, B-9000 Ghent, Belgium.
[Srama, Ralf; Sterken, Veerle J.] Univ Stuttgart, Inst Raumfahrtsyst, D-70174 Stuttgart, Germany.
[Sterken, Veerle J.] TU Braunschweig, IGEP, Braunschweig, Germany.
[Stroud, Rhonda M.] Naval Res Lab, Mat Sci & Technol Div, Washington, DC USA.
[Tsou, Peter] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Tsuchiyama, Akira] Osaka Univ, Dept Earth & Space Sci, Osaka, Japan.
RP Simionovici, AS (reprint author), Univ Grenoble, Observ Sci, Inst Sci Terre, Grenoble, France.
EM Alexandre.Simionovici@ujf-grenoble.fr
RI Sans Tresserras, Juan Angel/J-9362-2014; Leitner, Jan/A-7391-2015;
Hoppe, Peter/B-3032-2015; Bajt, Sasa/G-2228-2010; Stroud,
Rhonda/C-5503-2008;
OI Sans Tresserras, Juan Angel/0000-0001-9047-3992; Leitner,
Jan/0000-0003-3655-6273; Hoppe, Peter/0000-0003-3681-050X; Stroud,
Rhonda/0000-0001-5242-8015; Burchell, Mark/0000-0002-2680-8943
FU French "Centre National d'Etudes Spatiales" (CNES); NASA
FX A. Simionovici and L. Lemelle acknowledge support from the French
"Centre National d'Etudes Spatiales" (CNES). The Stardust mission was
supported by NASA as the fourth mission in the Discovery program.
NR 29
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U1 0
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PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 1086-9379
EI 1945-5100
J9 METEORIT PLANET SCI
JI Meteorit. Planet. Sci.
PD SEP
PY 2014
VL 49
IS 9
SI SI
BP 1612
EP 1625
DI 10.1111/maps.12208
PG 14
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA AQ6HT
UT WOS:000342912100006
ER
PT J
AU Flynn, GJ
Sutton, SR
Lai, B
Wirick, S
Allen, C
Anderson, D
Ansari, A
Bajt, S
Bastien, RK
Bassim, N
Bechtel, HA
Borg, J
Brenker, FE
Bridges, J
Brownlee, DE
Burchell, M
Burghammer, M
Butterworth, AL
Changela, H
Cloetens, P
Davis, AM
Doll, R
Floss, C
Frank, D
Gainsforth, Z
Grun, E
Heck, PR
Hillier, JK
Hoppe, P
Hudson, B
Huth, J
Hvide, B
Kearsley, A
King, AJ
Leitner, J
Lemelle, L
Leroux, H
Leonard, A
Lettieri, R
Marchant, W
Nittler, LR
Ogliore, R
Ong, WJ
Postberg, F
Price, MC
Sandford, SA
Tresseras, JAS
Schmitz, S
Schoonjans, T
Silversmit, G
Simionovici, A
Sole, VA
Srama, R
Stadermann, FJ
Stephan, T
Sterken, V
Stodolna, J
Stroud, RM
Trieloff, M
Tsou, P
Tsuchiyama, A
Tyliszczak, T
Vekemans, B
Vincze, L
Von Korff, J
Westphal, AJ
Wordsworth, N
Zevin, D
Zolensky, ME
AF Flynn, George J.
Sutton, Steven R.
Lai, Barry
Wirick, Sue
Allen, Carlton
Anderson, David
Ansari, Asna
Bajt, Sasa
Bastien, Ron K.
Bassim, Nabil
Bechtel, Hans A.
Borg, Janet
Brenker, Frank E.
Bridges, John
Brownlee, Donald E.
Burchell, Mark
Burghammer, Manfred
Butterworth, Anna L.
Changela, Hitesh
Cloetens, Peter
Davis, Andrew M.
Doll, Ryan
Floss, Christine
Frank, David
Gainsforth, Zack
Gruen, Eberhard
Heck, Philipp R.
Hillier, Jon K.
Hoppe, Peter
Hudson, Bruce
Huth, Joachim
Hvide, Brit
Kearsley, Anton
King, Ashley J.
Leitner, Jan
Lemelle, Laurence
Leroux, Hugues
Leonard, Ariel
Lettieri, Robert
Marchant, William
Nittler, Larry R.
Ogliore, Ryan
Ong, Wei Ja
Postberg, Frank
Price, Mark C.
Sandford, Scott A.
Tresseras, Juan-Angel Sans
Schmitz, Sylvia
Schoonjans, Tom
Silversmit, Geert
Simionovici, Alexandre
Sole, Vicente A.
Srama, Ralf
Stadermann, Frank J.
Stephan, Thomas
Sterken, Veerle
Stodolna, Julien
Stroud, Rhonda M.
Trieloff, Mario
Tsou, Peter
Tsuchiyama, Akira
Tyliszczak, Tolek
Vekemans, Bart
Vincze, Laszlo
Von Korff, Joshua
Westphal, Andrew J.
Wordsworth, Naomi
Zevin, Daniel
Zolensky, Michael E.
TI Stardust Interstellar Preliminary Examination VII: Synchrotron X-ray
fluorescence analysis of six Stardust interstellar candidates measured
with the Advanced Photon Source 2-ID-D microprobe
SO METEORITICS & PLANETARY SCIENCE
LA English
DT Article
ID COMET 81P/WILD-2; SOLAR-SYSTEM; DUST; ABUNDANCES; ELEMENTS
AB The NASA Stardust spacecraft exposed an aerogel collector to the interstellar dust passing through the solar system. We performed X-ray fluorescence element mapping and abundance measurements, for elements 19 <= Z <= 30, on six "interstellar candidates," potential interstellar impacts identified by Stardust@Home and extracted for analyses in picokeystones. One, I1044,3,33, showed no element hot-spots within the designated search area. However, we identified a nearby surface feature, consistent with the impact of a weak, high-speed particle having an approximately chondritic (CI) element abundance pattern, except for factor-of-ten enrichments in K and Zn and an S depletion. This hot-spot, containing approximately 10 fg of Fe, corresponds to an approximately 350 nm chondritic particle, small enough to be missed by Stardust@Home, indicating that other techniques may be necessary to identify all interstellar candidates. Only one interstellar candidate, I1004,1,2, showed a track. The terminal particle has large enrichments in S, Ti, Cr, Mn, Ni, Cu, and Zn relative to Fe-normalized CI values. It has high Al/Fe, but does not match the Ni/Fe range measured for samples of Al-deck material from the Stardust sample return capsule, which was within the field-of-view of the interstellar collector. A third interstellar candidate, I1075,1,25, showed an Al-rich surface feature that has a composition generally consistent with the Al-deck material, suggesting that it is a secondary particle. The other three interstellar candidates, I1001,1,16, I1001,2,17, and I1044,2,32, showed no impact features or tracks, but allowed assessment of submicron contamination in this aerogel, including Fe hot-spots having CI-like Ni/Fe ratios, complicating the search for CI-like interstellar/interplanetary dust.
C1 [Flynn, George J.] SUNY Coll Plattsburgh, Plattsburgh, NY 12901 USA.
[Sutton, Steven R.; Lai, Barry] Argonne Natl Lab, Adv Photon Source, Chicago, IL USA.
[Sutton, Steven R.; Wirick, Sue] Univ Chicago, CARS, Chicago, IL 60637 USA.
[Allen, Carlton; Bastien, Ron K.; Frank, David; Zolensky, Michael E.] NASA JSC, ARES, Houston, TX USA.
[Anderson, David; Butterworth, Anna L.; Gainsforth, Zack; Lettieri, Robert; Marchant, William; Stodolna, Julien; Von Korff, Joshua; Westphal, Andrew J.; Zevin, Daniel] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA USA.
[Ansari, Asna; Heck, Philipp R.; Hvide, Brit] Field Museum Nat Hist, Robert A Pritzker Ctr Meteorit & Polar Studies, Chicago, IL 60605 USA.
[Bajt, Sasa] DESY, Hamburg, Germany.
[Bassim, Nabil] Naval Res Lab, Washington, DC USA.
[Bechtel, Hans A.; Tyliszczak, Tolek] Lawrence Berkeley Lab, Adv Light Source, Berkeley, CA USA.
[Borg, Janet] IAS Orsay, Orsay, France.
[Brenker, Frank E.; Schmitz, Sylvia] Goethe Univ Frankfurt, Inst Geosci, Frankfurt, Germany.
[Bridges, John] Univ Leicester, Space Res Ctr, Leicester, Leics, England.
[Brownlee, Donald E.] Univ Washington, Dept Astron, Seattle, WA 98195 USA.
[Burchell, Mark; Price, Mark C.] Univ Kent, Canterbury CT2 7NZ, Kent, England.
[Burghammer, Manfred; Cloetens, Peter; Tresseras, Juan-Angel Sans; Sole, Vicente A.] European Synchrotron Radiat Facil, F-38043 Grenoble, France.
[Changela, Hitesh] George Washington Univ, Washington, DC USA.
[Davis, Andrew M.; Stephan, Thomas] Univ Chicago, Chicago, IL 60637 USA.
[Doll, Ryan; Floss, Christine; Leonard, Ariel; Ong, Wei Ja; Stadermann, Frank J.] Washington Univ, St Louis, MO USA.
[Gruen, Eberhard] Max Planck Inst Kernphys, D-69117 Heidelberg, Germany.
[Hillier, Jon K.; Postberg, Frank; Trieloff, Mario] Heidelberg Univ, Inst Geowissensch, Heidelberg, Germany.
[Hoppe, Peter; Huth, Joachim; Leitner, Jan] Max Planck Inst Chem, D-55128 Mainz, Germany.
[Kearsley, Anton] Nat Hist Museum, London SW7 5BD, England.
[King, Ashley J.] Univ Chicago, Chicago, IL 60637 USA.
[King, Ashley J.] Field Museum Nat Hist, Robert A Pritzker Ctr Meteorit & Polar Studies, Chicago, IL 60605 USA.
[Lemelle, Laurence] Ecole Normale Super Lyon, F-69364 Lyon, France.
[Leroux, Hugues] Univ Lille 1, UMR CNRS 8008, Lab Struct & Proprietes Etat Solide, F-59655 Villeneuve Dascq, France.
[Nittler, Larry R.] Carnegie Inst Sci, Washington, DC USA.
[Ogliore, Ryan] Univ Hawaii Manoa, Honolulu, HI 96822 USA.
[Sandford, Scott A.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Schoonjans, Tom; Silversmit, Geert; Vekemans, Bart; Vincze, Laszlo] Univ Ghent, B-9000 Ghent, Belgium.
[Simionovici, Alexandre] Univ Grenoble, Observ Sci, Inst Sci Terre, Grenoble, France.
[Srama, Ralf] Univ Stuttgart, Inst Raumfahrtsyst, D-70174 Stuttgart, Germany.
[Sterken, Veerle] Univ Stuttgart, D-70174 Stuttgart, Germany.
[Sterken, Veerle] TU Braunschweig, Inst Geophys & Extraterrestrial Phys, Braunschweig, Germany.
[Sterken, Veerle] Max Planck Inst Kernphys, D-69117 Heidelberg, Germany.
[Stroud, Rhonda M.] Naval Res Lab, Mat Sci & Technol Div, Washington, DC USA.
[Tsou, Peter] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Tsuchiyama, Akira] Osaka Univ, Osaka, Japan.
RP Flynn, GJ (reprint author), SUNY Coll Plattsburgh, Plattsburgh, NY 12901 USA.
EM flynngj@plattsburgh.edu
RI Bajt, Sasa/G-2228-2010; Sans Tresserras, Juan Angel/J-9362-2014;
Leitner, Jan/A-7391-2015; Hoppe, Peter/B-3032-2015
OI Burchell, Mark/0000-0002-2680-8943; Sans Tresserras, Juan
Angel/0000-0001-9047-3992; Leitner, Jan/0000-0003-3655-6273; Hoppe,
Peter/0000-0003-3681-050X
FU NASA; NASA Laboratory Analysis of Returned Samples research grant
[NNX11AE15G]; U.S. DOE [DE-AC02-06CH11357]; Department of Energy
(DOE)-Geosciences [DE-FG02-92ER14244]; DOE [DE-AC02-98CH10886]
FX The Stardust interstellar dust collection mission was supported by NASA
as the fourth mission in the Discovery program. This analytical work was
supported by a NASA Laboratory Analysis of Returned Samples research
grant NNX11AE15G (to G. J. F.). Use of the Advanced Photon Source, an
Office of Science User Facility operated for the U.S. Department of
Energy (DOE) Office of Science by Argonne National Laboratory, was
supported by the U.S. DOE under Contract No. DE-AC02-06CH11357. Portions
of this work were performed at Beamline X26A, National Synchrotron Light
Source (NSLS), Brookhaven National Laboratory. X26A is supported by the
Department of Energy (DOE)-Geosciences (DE-FG02-92ER14244 to The
University of Chicago-CARS). Use of the NSLS was supported by DOE under
Contract No. DE-AC02-98CH10886.
NR 20
TC 9
Z9 9
U1 0
U2 10
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 1086-9379
EI 1945-5100
J9 METEORIT PLANET SCI
JI Meteorit. Planet. Sci.
PD SEP
PY 2014
VL 49
IS 9
SI SI
BP 1626
EP 1644
DI 10.1111/maps.12144
PG 19
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA AQ6HT
UT WOS:000342912100007
ER
PT J
AU Gainsforth, Z
Brenker, FE
Simionovici, AS
Schmitz, S
Burghammer, M
Butterworth, AL
Cloetens, P
Lemelle, L
Tresserras, JAS
Schoonjans, T
Silversmit, G
Sole, VA
Vekemans, B
Vincze, L
Westphal, AJ
Allen, C
Anderson, D
Ansari, A
Bajt, S
Bastien, RK
Bassim, N
Bechtel, HA
Borg, J
Bridges, J
Brownlee, DE
Burchell, M
Changela, H
Davis, AM
Doll, R
Floss, C
Flynn, G
Fougeray, P
Frank, D
Grun, E
Heck, PR
Hillier, JK
Hoppe, P
Hudson, B
Huth, J
Hvide, B
Kearsley, A
King, AJ
Lai, B
Leitner, J
Leroux, H
Leonard, A
Lettieri, R
Marchant, W
Nittler, LR
Ogliore, R
Ong, WJ
Postberg, F
Price, MC
Sandford, SA
Srama, R
Stephan, T
Sterken, V
Stodolna, J
Stroud, RM
Sutton, S
Trieloff, M
Tsou, P
Tsuchiyama, A
Tyliszczak, T
Von Korff, J
Zevin, D
Zolensky, ME
AF Gainsforth, Zack
Brenker, Frank E.
Simionovici, Alexandre S.
Schmitz, Sylvia
Burghammer, Manfred
Butterworth, Anna L.
Cloetens, Peter
Lemelle, Laurence
Tresserras, Juan-Angel Sans
Schoonjans, Tom
Silversmit, Geert
Sole, Vicente A.
Vekemans, Bart
Vincze, Laszlo
Westphal, Andrew J.
Allen, Carlton
Anderson, David
Ansari, Asna
Bajt, Sasa
Bastien, Ron K.
Bassim, Nabil
Bechtel, Hans A.
Borg, Janet
Bridges, John
Brownlee, Donald E.
Burchell, Mark
Changela, Hitesh
Davis, Andrew M.
Doll, Ryan
Floss, Christine
Flynn, George
Fougeray, Patrick
Frank, David
Gruen, Eberhard
Heck, Philipp R.
Hillier, Jon K.
Hoppe, Peter
Hudson, Bruce
Huth, Joachim
Hvide, Brit
Kearsley, Anton
King, Ashley J.
Lai, Barry
Leitner, Jan
Leroux, Hugues
Leonard, Ariel
Lettieri, Robert
Marchant, William
Nittler, Larry R.
Ogliore, Ryan
Ong, Wei Ja
Postberg, Frank
Price, Mark C.
Sandford, Scott A.
Srama, Ralf
Stephan, Thomas
Sterken, Veerle
Stodolna, Julien
Stroud, Rhonda M.
Sutton, Steven
Trieloff, Mario
Tsou, Peter
Tsuchiyama, Akira
Tyliszczak, Tolek
Von Korff, Joshua
Zevin, Daniel
Zolensky, Michael E.
TI Stardust Interstellar Preliminary Examination VIII: Identification of
crystalline material in two interstellar candidates
SO METEORITICS & PLANETARY SCIENCE
LA English
DT Article
ID DUST PARTICLES; ORDER-DISORDER; AEROGEL; DIFFRACTION; GRAINS;
DIMENSIONS; COLLECTION; SILICATES; GRAPHITE; OLIVINES
AB Using synchrotron-based X-ray diffraction measurements, we identified crystalline material in two particles of extraterrestrial origin extracted from the Stardust Interstellar Dust Collector. The first particle, I1047,1,34 (Hylabrook), consisted of a mosaiced olivine grain approximately 1 mu m in size with internal strain fields up to 0.3%. The unit cell dimensions were a - 4.85 +/- 0.08 angstrom, b - 10.34 +/- 0.16 angstrom, c - 6.08 +/- 0.13 angstrom (2 sigma). The second particle, I1043,1,30 (Orion), contained an olivine grain approximate to 2 mu m in length and > 500 nm in width. It was polycrystalline with both mosaiced domains varying over approximate to 20 degrees and additional unoriented domains, and contained internal strain fields < 1%. The unit cell dimensions of the olivine were a = 4.76 +/- 0.05 angstrom, b = 10.23 +/- 0.10 angstrom, c = 5.99 +/- 0.06 angstrom (2 sigma), which limited the olivine to a forsteritic composition [Fo(65) (2 sigma). Orion also contained abundant spinel nanocrystals of unknown composition, but unit cell dimension a = 8.06 +/- 0.08 angstrom (2 sigma). Two additional crystalline phases were present and remained unidentified. An amorphous component appeared to be present in both these particles based on STXM and XRF results reported elsewhere.
C1 [Gainsforth, Zack; Butterworth, Anna L.; Westphal, Andrew J.; Anderson, David; Lettieri, Robert; Marchant, William; Stodolna, Julien; Von Korff, Joshua; Zevin, Daniel] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
[Brenker, Frank E.; Schmitz, Sylvia] Goethe Univ Frankfurt, Inst Geosci, Frankfurt, Germany.
[Simionovici, Alexandre S.] Univ Grenoble, Observ Sci, Inst Sci Terre, Grenoble, France.
[Burghammer, Manfred; Cloetens, Peter; Tresserras, Juan-Angel Sans; Sole, Vicente A.] European Synchrotron Radiat Facil, F-38043 Grenoble, France.
[Lemelle, Laurence] Ecole Normale Super Lyon, F-69364 Lyon, France.
[Schoonjans, Tom; Silversmit, Geert; Vekemans, Bart; Vincze, Laszlo] Univ Ghent, Dept Analyt Chem, B-9000 Ghent, Belgium.
[Allen, Carlton; Zolensky, Michael E.] NASA JSC, ARES, Houston, TX USA.
[Ansari, Asna; Heck, Philipp R.; Hvide, Brit] Field Museum Nat Hist, Chicago, IL 60605 USA.
[Bajt, Sasa] DESY, Hamburg, Germany.
[Bastien, Ron K.; Frank, David] NASA JSC, ESCG, Houston, TX USA.
[Bassim, Nabil; Stroud, Rhonda M.] Naval Res Lab, Washington, DC USA.
[Bechtel, Hans A.; Tyliszczak, Tolek] Lawrence Berkeley Lab, Adv Light Source, Berkeley, CA USA.
[Borg, Janet] IAS Orsay, Orsay, France.
[Bridges, John] Univ Leicester, Space Res Ctr, Leicester, Leics, England.
[Brownlee, Donald E.] Univ Washington, Dept Astron, Seattle, WA 98195 USA.
[Burchell, Mark; Price, Mark C.] Univ Kent, Sch Phys Sci, Canterbury, Kent, England.
[Changela, Hitesh] Univ New Mexico, Dept Earth & Planetary Sci, Albuquerque, NM 87131 USA.
[Davis, Andrew M.; Stephan, Thomas] Univ Chicago, Dept Geophys Sci, Chicago, IL 60637 USA.
[Doll, Ryan; Floss, Christine; Leonard, Ariel; Ong, Wei Ja] Washington Univ, Dept Phys, St Louis, MO 63130 USA.
[Flynn, George; Sterken, Veerle] SUNY Coll Plattsburgh, Plattsburgh, NY 12901 USA.
[Fougeray, Patrick] Chigy, Burgundy, France.
[Gruen, Eberhard] Max Planck Inst Kernphys, D-69117 Heidelberg, Germany.
[Postberg, Frank; Trieloff, Mario] Heidelberg Univ, Inst Geowissensch, Heidelberg, Germany.
[Hoppe, Peter; Huth, Joachim; Leitner, Jan] Max Planck Inst Chem, D-55128 Mainz, Germany.
[Kearsley, Anton; King, Ashley J.] Nat Hist Museum, London SW7 5BD, England.
[Lai, Barry; Sutton, Steven] Argonne Natl Lab, Adv Photon Source, Chicago, IL USA.
[Leroux, Hugues] Univ Lille 1, Lille, France.
[Nittler, Larry R.] Carnegie Inst Sci, Washington, DC USA.
[Ogliore, Ryan] Univ Hawaii Manoa, Honolulu, HI 96822 USA.
[Hillier, Jon K.; Sandford, Scott A.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Srama, Ralf; Sterken, Veerle] Univ Stuttgart, IRS, D-70174 Stuttgart, Germany.
[Sterken, Veerle] TU Braunschweig, IGEP, Braunschweig, Germany.
[Tsou, Peter] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Tsuchiyama, Akira] Osaka Univ, Osaka, Japan.
RP Gainsforth, Z (reprint author), Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
EM zackg@ssl.berkeley.edu
RI Stroud, Rhonda/C-5503-2008; Leitner, Jan/A-7391-2015; Hoppe,
Peter/B-3032-2015; Bajt, Sasa/G-2228-2010
OI Stroud, Rhonda/0000-0001-5242-8015; Burchell, Mark/0000-0002-2680-8943;
Leitner, Jan/0000-0003-3655-6273; Hoppe, Peter/0000-0003-3681-050X;
FU NASA [NNX09AC36G]; Office of Science, Office of Basic Energy Sciences,
U.S. Department of Energy [DE-AC02-05CH11231]
FX Zack Gainsforth, Andrew J. Westphal, Anna L. Butterworth were supported
by NASA grant NNX09AC36G. The operations of the Advanced Light Source at
Lawrence Berkeley National Laboratory are supported by the Director,
Office of Science, Office of Basic Energy Sciences, U.S. Department of
Energy under contract number DE-AC02-05CH11231.
NR 54
TC 7
Z9 7
U1 0
U2 7
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 1086-9379
EI 1945-5100
J9 METEORIT PLANET SCI
JI Meteorit. Planet. Sci.
PD SEP
PY 2014
VL 49
IS 9
SI SI
BP 1645
EP 1665
DI 10.1111/maps.12148
PG 21
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA AQ6HT
UT WOS:000342912100008
ER
PT J
AU Postberg, F
Hillier, JK
Armes, SP
Bugiel, S
Butterworth, A
Dupin, D
Fielding, LA
Fujii, S
Gainsforth, Z
Grun, E
Li, YW
Srama, R
Sterken, V
Stodolna, J
Trieloff, M
Westphal, A
Achilles, C
Allen, C
Ansari, A
Bajt, S
Bassim, N
Bastien, RK
Bechtel, HA
Borg, J
Brenker, F
Bridges, J
Brownlee, DE
Burchell, M
Burghammer, M
Changela, H
Cloetens, P
Davis, A
Doll, R
Floss, C
Flynn, G
Frank, D
Heck, PR
Hoppe, P
Huss, G
Huth, J
Kearsley, A
King, AJ
Lai, B
Leitner, J
Lemelle, L
Leonard, A
Leroux, H
Lettieri, R
Marchant, W
Nittler, LR
Ogliore, R
Ong, WJ
Price, MC
Sandford, SA
Tressaras, JAS
Schmitz, S
Schoonjans, T
Schreiber, K
Silversmit, G
Simionovici, A
Sole, VA
Stadermann, F
Stephan, T
Stroud, RM
Sutton, S
Tsou, P
Tsuchiyama, A
Tyliczszak, T
Vekemans, B
Vincze, L
Zevin, D
Zolensky, ME
AF Postberg, F.
Hillier, J. K.
Armes, S. P.
Bugiel, S.
Butterworth, A.
Dupin, D.
Fielding, L. A.
Fujii, S.
Gainsforth, Z.
Gruen, E.
Li, Y. W.
Srama, R.
Sterken, V.
Stodolna, J.
Trieloff, M.
Westphal, A.
Achilles, C.
Allen, C.
Ansari, A.
Bajt, S.
Bassim, N.
Bastien, R. K.
Bechtel, H. A.
Borg, J.
Brenker, F.
Bridges, J.
Brownlee, D. E.
Burchell, M.
Burghammer, M.
Changela, H.
Cloetens, P.
Davis, A.
Doll, R.
Floss, C.
Flynn, G.
Frank, D.
Heck, P. R.
Hoppe, P.
Huss, G.
Huth, J.
Kearsley, A.
King, A. J.
Lai, B.
Leitner, J.
Lemelle, L.
Leonard, A.
Leroux, H.
Lettieri, R.
Marchant, W.
Nittler, L. R.
Ogliore, R.
Ong, W. J.
Price, M. C.
Sandford, S. A.
Tressaras, J. -A. Sans
Schmitz, S.
Schoonjans, T.
Schreiber, K.
Silversmit, G.
Simionovici, A.
Sole, V. A.
Stadermann, F.
Stephan, T.
Stroud, R. M.
Sutton, S.
Tsou, P.
Tsuchiyama, A.
Tyliczszak, T.
Vekemans, B.
Vincze, L.
Zevin, D.
Zolensky, M. E.
TI Stardust Interstellar Preliminary Examination IX: High-speed
interstellar dust analog capture in Stardust flight-spare aerogel
SO METEORITICS & PLANETARY SCIENCE
LA English
DT Article
ID COMET 81P/WILD 2; IMPACT FEATURES; MICROPARTICLES; PARTICLES; TRACKS
AB The NASA Stardust mission used silica aerogel slabs to slowly decelerate and capture impinging cosmic dust particles for return to Earth. During this process, impact tracks are generated along the trajectory of the particle into the aerogel. It is believed that the morphology and dimensions of these tracks, together with the state of captured grains at track termini, may be linked to the size, velocity, and density of the impacting cosmic dust grain. Here, we present the results of laboratory hypervelocity impact experiments, during which cosmic dust analog particles (diameters of between 0.2 and 0.4 mu m), composed of olivine, orthopyroxene, or an organic polymer, were accelerated onto Stardust flight-spare low-density (approximately 0.01 g cm(-3)) silica aerogel. The impact velocities (3-21 km s(-1)) were chosen to simulate the range of velocities expected during Stardust's interstellar dust (ISD) collection phases. Track lengths and widths, together with the success of particle capture, are analyzed as functions of impact velocity and particle composition, density, and size. Captured terminal particles from low-density organic projectiles become undetectable at lower velocities than those from similarly sized, denser mineral particles, which are still detectable (although substantially altered by the impact process) at 15 km s(-1). The survival of these terminal particles, together with the track dimensions obtained during low impact speed capture of small grains in the laboratory, indicates that two of the three best Stardust candidate extraterrestrial grains were actually captured at speeds much lower than predicted. Track length and diameters are, in general, more sensitive to impact velocities than previously expected, which makes tracks of particles with diameters of 0.4 mu m and below hard to identify at low capture speeds (<10 km s(-1)). Therefore, although captured intact, the majority of the interstellar dust grains returned to Earth by Stardust remain to be found.
C1 [Postberg, F.; Bugiel, S.; Li, Y. W.; Srama, R.; Sterken, V.] Univ Stuttgart, Inst Raumfahrtsyst, Stuttgart, Germany.
[Postberg, F.; Hillier, J. K.; Trieloff, M.] Heidelberg Univ, Inst Geowissensch, D-69115 Heidelberg, Germany.
[Armes, S. P.; Dupin, D.; Fielding, L. A.; Fujii, S.] Univ Sheffield, Dept Chem, Sheffield, S Yorkshire, England.
[Bugiel, S.; Gruen, E.; Li, Y. W.; Sterken, V.] Max Planck Inst Kernphys, D-69117 Heidelberg, Germany.
[Butterworth, A.; Gainsforth, Z.; Stodolna, J.; Westphal, A.; Lettieri, R.; Marchant, W.; Zevin, D.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA USA.
[Gruen, E.] Univ Colorado, LASP, Boulder, CO 80309 USA.
[Li, Y. W.] Harbin Inst Technol, Sch Mat Sci & Engn, Harbin 150006, Peoples R China.
[Sterken, V.] Tech Univ Carolo Wilhelmina Braunschweig, IGEP, D-38106 Braunschweig, Germany.
[Achilles, C.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA.
[Allen, C.; Bastien, R. K.; Frank, D.; Zolensky, M. E.] NASA, Lyndon B Johnson Space Ctr, ARES, Houston, TX 77058 USA.
[Ansari, A.; Davis, A.; King, A. J.; Stephan, T.] Univ Chicago, Chicago, IL 60637 USA.
[Bajt, S.] DESY, Hamburg, Germany.
[Bassim, N.; Changela, H.; Stroud, R. M.] Naval Res Lab, Washington, DC USA.
[Bechtel, H. A.; Tyliczszak, T.] Lawrence Berkeley Lab, Adv Light Source, Berkeley, CA USA.
[Borg, J.] IAS Orsay, Orsay, France.
[Brenker, F.; Schmitz, S.] Univ Frankfurt Main, Inst Geowissensch, Frankfurt, Germany.
[Bridges, J.] Univ Leicester, Space Res Ctr, Leicester, Leics, England.
[Brownlee, D. E.] Univ Washington, Dept Astron, Seattle, WA 98195 USA.
[Burchell, M.; Price, M. C.] Univ Kent, Sch Phys Sci, Canterbury, Kent, England.
[Burghammer, M.; Cloetens, P.; Tressaras, J. -A. Sans; Sole, V. A.] European Synchrotron Radiat Facil, F-38043 Grenoble, France.
[Changela, H.] George Washington Univ, Washington, DC USA.
[Doll, R.; Floss, C.; Leonard, A.; Ong, W. J.; Schreiber, K.; Stadermann, F.] Washington Univ, St Louis, MO USA.
[Flynn, G.] SUNY Coll Plattsburgh, Plattsburgh, NY 12901 USA.
[Heck, P. R.] Field Museum Nat Hist, Robert A Pritzker Ctr Meteorit & Polar Studies, Chicago, IL 60605 USA.
[Hoppe, P.; Huth, J.; Leitner, J.] Max Planck Inst Chem, D-55128 Mainz, Germany.
[Huss, G.; Ogliore, R.] Univ Hawaii Manoa, Honolulu, HI 96822 USA.
[Kearsley, A.] Nat Hist Museum, London SW7 5BD, England.
[Lai, B.; Sutton, S.] Argonne Natl Lab, Adv Photon Source, Chicago, IL USA.
[Lemelle, L.] Ecole Normale Super Lyon, F-69364 Lyon, France.
[Leroux, H.] Univ Lille 1, Lille, France.
[Nittler, L. R.] Carnegie Inst Sci, Washington, DC USA.
[Sandford, S. A.] NASA Ames Res Ctr, Moffett Field, CA USA.
[Schoonjans, T.; Silversmit, G.; Vekemans, B.; Vincze, L.] Univ Ghent, B-9000 Ghent, Belgium.
[Simionovici, A.] Univ Grenoble, Observ Sci, Inst Sci Terre, Grenoble, France.
[Tsou, P.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Tsuchiyama, A.] Osaka Univ, Osaka, Japan.
RP Postberg, F (reprint author), Univ Stuttgart, Inst Raumfahrtsyst, Stuttgart, Germany.
EM postberg@irs.uni-stuttgart.de
RI Fielding, Lee/B-8440-2011; Stroud, Rhonda/C-5503-2008; Leitner,
Jan/A-7391-2015; Hoppe, Peter/B-3032-2015; Bajt, Sasa/G-2228-2010;
OI Fielding, Lee/0000-0002-4958-1155; Stroud, Rhonda/0000-0001-5242-8015;
Burchell, Mark/0000-0002-2680-8943; Armes, Steven/0000-0002-8289-6351;
Sans Tresserras, Juan Angel/0000-0001-9047-3992; Leitner,
Jan/0000-0003-3655-6273; Hoppe, Peter/0000-0003-3681-050X; Fujii,
Syuji/0000-0003-2562-9502
FU NASA [NNX09AC36G, NNH11AQ61I]; Office of Science, Office of Basic Energy
Sciences, of the U.S. Department of Energy [DE-AC02- 05CH11231]; U.S.
Department of Energy, Office of Science, Office of Basic Energy Sciences
[DE-AC02-98CH10886]; DFG [1385]; Klaus Tschira Stiftung GmbH
FX The ISPE consortium gratefully acknowledge the NASA Discovery Program
for Stardust, the fourth NASA Discovery mission. AJW, ALB, ZG, RL, DZ,
WM and JVK were supported by NASA grant NNX09AC36G. We thank Steve Boggs
for astrophysical soft x-ray spectra. RMS, HCG and NDB were supported by
NASA grant NNH11AQ61I. 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. Use of
the National Synchrotron Light Source, Brookhaven National Laboratory,
was supported by the U.S. Department of Energy, Office of Science,
Office of Basic Energy Sciences, under Contract No. DE-AC02-98CH10886.;
FP, JKH, RS and MT acknowledge funding by DFG special priority program
1385 "The First 10 Million years of the Solar System" and the support by
Klaus Tschira Stiftung GmbH.
NR 28
TC 11
Z9 11
U1 2
U2 23
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 1086-9379
EI 1945-5100
J9 METEORIT PLANET SCI
JI Meteorit. Planet. Sci.
PD SEP
PY 2014
VL 49
IS 9
SI SI
BP 1666
EP 1679
DI 10.1111/maps.12173
PG 14
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA AQ6HT
UT WOS:000342912100009
ER
PT J
AU Sterken, VJ
Westphal, AJ
Altobelli, N
Grun, E
Hillier, JK
Postberg, F
Srama, R
Allen, C
Anderson, D
Ansari, A
Bajt, S
Bastien, RS
Bassim, N
Bechtel, HA
Borg, J
Brenker, FE
Bridges, J
Brownlee, DE
Burchell, M
Burghammer, M
Butterworth, AL
Changela, H
Cloetens, P
Davis, AM
Doll, R
Floss, C
Flynn, G
Frank, D
Gainsforth, Z
Heck, PR
Hoppe, P
Hudson, B
Huth, J
Hvide, B
Kearsley, A
King, AJ
Lai, B
Leitner, J
Lemelle, L
Leroux, H
Leonard, A
Lettieri, R
Marchant, W
Nittler, LR
Ogliore, R
Ong, WJ
Price, MC
Sandford, SA
Tresseras, JAS
Schmitz, S
Schoonjans, T
Silversmit, G
Simionovici, A
Sole, VA
Stephan, T
Stodolna, J
Stroud, RM
Sutton, S
Trieloff, M
Tsou, P
Tsuchiyama, A
Tyliszczak, T
Vekemans, B
Vincze, L
Von Korff, J
Wordsworth, N
Zevin, D
Zolensky, ME
AF Sterken, Veerle J.
Westphal, Andrew J.
Altobelli, Nicolas
Gruen, Eberhard
Hillier, Jon K.
Postberg, Frank
Srama, Ralf
Allen, Carlton
Anderson, David
Ansari, Asna
Bajt, Sasa
Bastien, Ron S.
Bassim, Nabil
Bechtel, Hans A.
Borg, Janet
Brenker, Frank E.
Bridges, John
Brownlee, Donald E.
Burchell, Mark
Burghammer, Manfred
Butterworth, Anna L.
Changela, Hitesh
Cloetens, Peter
Davis, Andrew M.
Doll, Ryan
Floss, Christine
Flynn, George
Frank, David
Gainsforth, Zack
Heck, Philipp R.
Hoppe, Peter
Hudson, Bruce
Huth, Joachim
Hvide, Brit
Kearsley, Anton
King, Ashley J.
Lai, Barry
Leitner, Jan
Lemelle, Laurence
Leroux, Hugues
Leonard, Ariel
Lettieri, Robert
Marchant, William
Nittler, Larry R.
Ogliore, Ryan
Ong, Wei Ja
Price, Mark C.
Sandford, S. A.
Tresseras, Juan-Angel Sans
Schmitz, Sylvia
Schoonjans, Tom
Silversmit, Geert
Simionovici, Alexandre
Sole, Vicente A.
Stephan, Thomas
Stodolna, Julien
Stroud, Rhonda M.
Sutton, Steven
Trieloff, Mario
Tsou, Peter
Tsuchiyama, Akira
Tyliszczak, Tolek
Vekemans, Bart
Vincze, Laszlo
Von Korff, Joshua
Wordsworth, Naomi
Zevin, Daniel
Zolensky, Michael E.
TI Stardust Interstellar Preliminary Examination X: Impact speeds and
directions of interstellar grains on the Stardust dust collector
SO METEORITICS & PLANETARY SCIENCE
LA English
DT Article
ID RADIATION PRESSURE; SIZE DISTRIBUTION; SAMPLE RETURN; EARTH;
HELIOSPHERE; PARTICLES; AEROGEL; MATTER; SARIM
AB On the basis of an interstellar dust model compatible with Ulysses and Galileo observations, we calculate and predict the trajectories of interstellar dust (ISD) in the solar system and the distribution of the impact speeds, directions, and flux of ISD particles on the Stardust Interstellar Dust Collector during the two collection periods of the mission. We find that the expected impact velocities are generally low (<10 km s(-1)) for particles with the ratio of the solar radiation pressure force to the solar gravitational force beta > 1, and that some of the particles will impact on the cometary side of the collector. If we assume astronomical silicates for particle material and a density of 2 g cm(-3), and use the Ulysses measurements and the ISD trajectory simulations, we conclude that the total number of (detectable) captured ISD particles may be on the order of 50. In companion papers in this volume, we report the discovery of three interstellar dust candidates in the Stardust aerogel tiles. The impact directions and speeds of these candidates are consistent with those calculated from our ISD propagation model, within the uncertainties of the model and of the observations.
C1 [Sterken, Veerle J.] Univ Stuttgart, Inst Raumfahrtsyst, D-70569 Stuttgart, Germany.
[Sterken, Veerle J.] Tech Univ Carolo Wilhelmina Braunschweig, Inst Geophys & Extreterr Phys, D-38106 Braunschweig, Germany.
[Westphal, Andrew J.; Anderson, David; Butterworth, Anna L.; Gainsforth, Zack; Lettieri, Robert; Marchant, William; Stodolna, Julien; Von Korff, Joshua; Zevin, Daniel] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
[Altobelli, Nicolas] European Space Agcy, Madrid, Spain.
[Gruen, Eberhard] Max Planck Inst Kernphys, D-69117 Heidelberg, Germany.
[Hillier, Jon K.; Postberg, Frank; Trieloff, Mario] Heidelberg Univ, Inst Geowissensch, Heidelberg, Germany.
[Srama, Ralf] Univ Stuttgart, Inst Raumfahrtsyst, D-70174 Stuttgart, Germany.
[Allen, Carlton; Zolensky, Michael E.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA.
[Ansari, Asna; Hvide, Brit] Field Museum Nat Hist, Robert A Pritzker Ctr Meteorit & Polar Studies, Chicago, IL 60605 USA.
[Bajt, Sasa] DESY, Hamburg, Germany.
[Bastien, Ron S.; Frank, David] NASA, Lyndon B Johnson Space Ctr, Engn & Sci Contract Grp, Houston, TX 77058 USA.
[Bassim, Nabil] Naval Res Lab, Washington, DC USA.
[Bechtel, Hans A.; Tyliszczak, Tolek] Lawrence Berkeley Lab, Adv Light Source, Berkeley, CA USA.
[Borg, Janet] Inst Astrophys Spatiale, Orsay, France.
[Brenker, Frank E.] Goethe Univ Frankfurt, Inst Geosci, Frankfurt, Germany.
[Bridges, John] Univ Leicester, Space Res Ctr, Leicester, Leics, England.
[Brownlee, Donald E.] Univ Washington, Dept Astron, Seattle, WA 98195 USA.
[Burchell, Mark; Price, Mark C.] Univ Kent, Sch Phys Sci, Canterbury, Kent, England.
[Burghammer, Manfred; Cloetens, Peter; Tresseras, Juan-Angel Sans; Sole, Vicente A.] European Synchrotron Radiat Facil, F-38043 Grenoble, France.
[Changela, Hitesh] Univ New Mexico, Dept Earth & Planetary Sci, Albuquerque, NM 87131 USA.
[Davis, Andrew M.; Stephan, Thomas] Univ Chicago, Dept Geophys Sci, Chicago, IL 60637 USA.
[Doll, Ryan; Floss, Christine; Leonard, Ariel; Ong, Wei Ja] Washington Univ, Dept Phys, St Louis, MO 63130 USA.
[Flynn, George] SUNY Coll Plattsburgh, Plattsburgh, NY 12901 USA.
[Heck, Philipp R.] Field Museum Nat Hist, Chicago, IL 60605 USA.
[Hoppe, Peter; Huth, Joachim; Leitner, Jan] Max Planck Inst Chem, D-55128 Mainz, Germany.
[Kearsley, Anton] Nat Hist Museum, London SW7 5BD, England.
[King, Ashley J.] Univ Chicago, Chicago, IL 60637 USA.
[King, Ashley J.] Field Museum Nat Hist, Robert A Pritzker Ctr Meteorit & Polar Studies, Chicago, IL 60605 USA.
[Lai, Barry; Sutton, Steven] Argonne Natl Lab, Adv Photon Source, Chicago, IL USA.
[Lemelle, Laurence] Ecole Normale Super Lyon, F-69364 Lyon, France.
[Leroux, Hugues] Univ Sci & Tech Lille, Lille, France.
[Nittler, Larry R.] Carnegie Inst Sci, Washington, DC USA.
[Ogliore, Ryan] Univ Hawaii Manoa, Hawaii Inst Geophys & Planetol, Honolulu, HI 96822 USA.
[Sandford, S. A.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Schmitz, Sylvia] Univ Frankfurt Main, Inst Geowissensch, Frankfurt, Germany.
[Schoonjans, Tom; Silversmit, Geert; Vekemans, Bart; Vincze, Laszlo] Univ Ghent, Dept Analyt Chem, B-9000 Ghent, Belgium.
[Simionovici, Alexandre] Univ Grenoble, Observ Sci, Inst Sci Terre, Grenoble, France.
[Stroud, Rhonda M.] Naval Res Lab, Mat Sci & Technol Div, Washington, DC USA.
[Tsou, Peter] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Tsuchiyama, Akira] Osaka Univ, Dept Earth & Space Sci, Osaka, Japan.
RP Sterken, VJ (reprint author), Int Space Sci Inst ISSI, Hallerstr 6, CH-3012 Bern, Switzerland.
EM veerle.sterken@issibern.ch
RI Sans Tresserras, Juan Angel/J-9362-2014; Bajt, Sasa/G-2228-2010; Stroud,
Rhonda/C-5503-2008; Leitner, Jan/A-7391-2015; Hoppe, Peter/B-3032-2015
OI Sans Tresserras, Juan Angel/0000-0001-9047-3992; Stroud,
Rhonda/0000-0001-5242-8015; Burchell, Mark/0000-0002-2680-8943; Leitner,
Jan/0000-0003-3655-6273; Hoppe, Peter/0000-0003-3681-050X
FU NASA [NNX09AC36G, NNH11AQ61I]; ESA; Office of Science, Office of Basic
Energy Sciences, of the U.S. Department of Energy [DE-AC02-05CH11231];
U.S. Department of Energy, Office of Science, Office of Basic Energy
Sciences [DE-AC02-98CH10886]
FX We thank the reviewers and the AE Christian Koeberl, for their
thoughtful reviews that greatly improved this manuscript. We also thank
the AE John Bradley for his critical input and time and effort spent
reviewing the ISPE manuscripts. The ISPE consortium gratefully
acknowledge the NASA Discovery Program for Stardust, the fourth NASA
Discovery mission. AJW, ALB, ZG, RL, DZ, WM, and JVK were supported by
NASA grant NNX09AC36G. RMS, HCG, and NDB were supported by NASA grant
NNH11AQ61I. VJS acknowledges support from ESA. 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. Use of the National Synchrotron Light Source,
Brookhaven National Laboratory, was supported by the U.S. Department of
Energy, Office of Science, Office of Basic Energy Sciences, under
Contract No. DE-AC02-98CH10886.
NR 37
TC 15
Z9 15
U1 0
U2 12
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 1086-9379
EI 1945-5100
J9 METEORIT PLANET SCI
JI Meteorit. Planet. Sci.
PD SEP
PY 2014
VL 49
IS 9
SI SI
BP 1680
EP 1697
DI 10.1111/maps.12219
PG 18
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA AQ6HT
UT WOS:000342912100010
ER
PT J
AU Stroud, RM
Allen, C
Ansari, A
Anderson, D
Bajt, S
Bassim, N
Bastien, RS
Bechtel, HA
Borg, J
Brenker, FE
Bridges, J
Brownlee, DE
Burchell, M
Burghammer, M
Butterworth, AL
Changela, H
Cloetens, P
Davis, AM
Doll, R
Floss, C
Flynn, G
Frank, DR
Gainsforth, Z
Grun, E
Heck, PR
Hillier, JK
Hoppe, P
Huth, J
Hvide, B
Kearsley, A
King, AJ
Kotula, P
Lai, B
Leitner, J
Lemelle, L
Leroux, H
Leonard, A
Lettieri, R
Marchant, W
Nittler, LR
Ogliore, R
Ong, WJ
Postberg, F
Price, MC
Sandford, SA
Tresseras, JAS
Schmitz, S
Schoonjans, T
Schreiber, K
Silversmit, G
Simionovici, AS
Sole, VA
Srama, R
Stephan, T
Sterken, VJ
Stodolna, J
Sutton, S
Trieloff, M
Tsou, P
Tsuchiyama, A
Tyliszczak, T
Vekemans, B
Vincze, L
Westphal, AJ
Von Korff, J
Zevin, D
Zolensky, ME
AF Stroud, Rhonda M.
Allen, Carlton
Ansari, Asna
Anderson, David
Bajt, Sasa
Bassim, Nabil
Bastien, Ron S.
Bechtel, Hans A.
Borg, Janet
Brenker, Frank E.
Bridges, John
Brownlee, Donald E.
Burchell, Mark
Burghammer, Manfred
Butterworth, Anna L.
Changela, Hitesh
Cloetens, Peter
Davis, Andrew M.
Doll, Ryan
Floss, Christine
Flynn, George
Frank, David R.
Gainsforth, Zack
Gruen, Eberhard
Heck, Philipp R.
Hillier, Jon K.
Hoppe, Peter
Huth, Joachim
Hvide, Brit
Kearsley, Anton
King, Ashley J.
Kotula, Paul
Lai, Barry
Leitner, Jan
Lemelle, Laurence
Leroux, Hugues
Leonard, Ariel
Lettieri, Robert
Marchant, William
Nittler, Larry R.
Ogliore, Ryan
Ong, Wei Jia
Postberg, Frank
Price, Mark C.
Sandford, Scott A.
Tresseras, Juan-Angel Sans
Schmitz, Sylvia
Schoonjans, Tom
Schreiber, Kate
Silversmit, Geert
Simionovici, Alexandre S.
Sole, Vicente A.
Srama, Ralf
Stephan, Thomas
Sterken, Veerle J.
Stodolna, Julien
Sutton, Steven
Trieloff, Mario
Tsou, Peter
Tsuchiyama, Akira
Tyliszczak, Tolek
Vekemans, Bart
Vincze, Laszlo
Westphal, Andrew J.
Von Korff, Joshua
Zevin, Daniel
Zolensky, Michael E.
TI Stardust Interstellar Preliminary Examination XI: Identification and
elemental analysis of impact craters on Al foils from the Stardust
Interstellar Dust Collector
SO METEORITICS & PLANETARY SCIENCE
LA English
DT Article
ID TRANSMISSION ELECTRON-MICROSCOPY; COMET 81P/WILD 2; ISOTOPIC
COMPOSITIONS; ALUMINUM FOILS; RESIDUES; FEATURES; AEROGEL; MORPHOLOGY;
MISSION; MATTER
AB The Stardust Interstellar Preliminary Examination team analyzed thirteen Al foils from the NASA Stardust interstellar collector tray in order to locate candidate interstellar dust (ISD) grain impacts. Scanning electron microscope (SEM) images reveal that the foils possess abundant impact crater and crater-like features. Elemental analyses of the crater features, with Auger electron spectroscopy, SEM-based energy dispersive X-ray (EDX) spectroscopy, and scanning transmission electron microscope-based EDX spectroscopy, demonstrate that the majority are either the result of impacting debris fragments from the spacecraft solar panels, or intrinsic defects in the foil. The elemental analyses also reveal that four craters contain residues of a definite extraterrestrial origin, either as interplanetary dust particles or ISD particles. These four craters are designated level 2 interstellar candidates, based on the crater shapes indicative of hypervelocity impacts and the residue compositions inconsistent with spacecraft debris.
C1 [Stroud, Rhonda M.; Bassim, Nabil; Changela, Hitesh] Naval Res Lab, Mat Sci & Technol Div, Washington, DC 20375 USA.
[Allen, Carlton; Zolensky, Michael E.] NASA, Lyndon B Johnson Space Ctr, ARES, Houston, TX 77058 USA.
[Ansari, Asna; Heck, Philipp R.; Hvide, Brit; Marchant, William] Field Museum Nat Hist, Robert A Pritzker Ctr Meteorit & Polar Studies, Chicago, IL 60605 USA.
[Anderson, David; Butterworth, Anna L.; Gainsforth, Zack; Lettieri, Robert; Stodolna, Julien; Westphal, Andrew J.; Von Korff, Joshua; Zevin, Daniel] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA USA.
[Bajt, Sasa] DESY, Hamburg, Germany.
[Bastien, Ron S.; Frank, David R.] NASA, Lyndon B Johnson Space Ctr, JETS, Houston, TX 77058 USA.
[Bechtel, Hans A.; Tyliszczak, Tolek] Lawrence Berkeley Lab, Adv Light Source, Berkeley, CA USA.
[Borg, Janet] IAS Orsay, Orsay, France.
[Brenker, Frank E.; Schmitz, Sylvia] Goethe Univ Frankfurt, Inst Geowissensch, Frankfurt, Germany.
[Bridges, John] Univ Leicester, Space Res Ctr, Leicester, Leics, England.
[Brownlee, Donald E.] Univ Washington, Dept Astron, Seattle, WA 98195 USA.
[Burchell, Mark; Price, Mark C.] Univ Kent, Canterbury, Kent, England.
[Burghammer, Manfred; Cloetens, Peter; Tresseras, Juan-Angel Sans; Sole, Vicente A.] European Synchrotron Radiat Facil, F-38043 Grenoble, France.
[Changela, Hitesh] George Washington Univ, Washington, DC USA.
[Davis, Andrew M.; King, Ashley J.; Stephan, Thomas] Univ Chicago, Chicago, IL 60637 USA.
[Doll, Ryan; Floss, Christine; Leonard, Ariel; Ong, Wei Jia; Schreiber, Kate] Washington Univ, St Louis, MO USA.
[Flynn, George] SUNY Coll Plattsburgh, Plattsburgh, NY 12901 USA.
[Gruen, Eberhard; Srama, Ralf] Max Planck Inst Kernphys, D-69117 Heidelberg, Germany.
[Hillier, Jon K.; Postberg, Frank; Trieloff, Mario] Heidelberg Univ, Inst Geowissensch, Heidelberg, Germany.
[Hoppe, Peter; Huth, Joachim; Leitner, Jan] Max Planck Inst Chem, D-55128 Mainz, Germany.
[Kearsley, Anton] Nat Hist Museum, London SW7 5BD, England.
[Kotula, Paul] Sandia Natl Labs, Albuquerque, NM USA.
[Lai, Barry; Sutton, Steven] Argonne Natl Lab, Adv Photon Source, Chicago, IL USA.
[Lemelle, Laurence] ENS, Lyon, France.
[Leroux, Hugues] Univ Sci & Techol Lille, Lille, France.
[Nittler, Larry R.] Carnegie Inst Sci, Washington, DC USA.
[Ogliore, Ryan] Univ Hawaii Manoa, Honolulu, HI 96822 USA.
[Sandford, Scott A.; Vincze, Laszlo] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Schoonjans, Tom; Silversmit, Geert; Vekemans, Bart] Univ Ghent, B-9000 Ghent, Belgium.
[Simionovici, Alexandre S.] Univ Grenoble, Observ Sci, Inst Sci Terre, Grenoble, France.
[Srama, Ralf] TU Braunschweig, IGEP, Braunschweig, Germany.
[Sterken, Veerle J.] Univ Stuttgart, IRS, D-70174 Stuttgart, Germany.
[Tsou, Peter] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Tsuchiyama, Akira] Osaka Univ, Osaka, Japan.
RP Stroud, RM (reprint author), Naval Res Lab, Mat Sci & Technol Div, Washington, DC 20375 USA.
EM stroud@nrl.navy.mil
RI Sans Tresserras, Juan Angel/J-9362-2014; Kotula, Paul/A-7657-2011;
Leitner, Jan/A-7391-2015; Hoppe, Peter/B-3032-2015; Bajt,
Sasa/G-2228-2010; Stroud, Rhonda/C-5503-2008;
OI Sans Tresserras, Juan Angel/0000-0001-9047-3992; Kotula,
Paul/0000-0002-7521-2759; Leitner, Jan/0000-0003-3655-6273; Hoppe,
Peter/0000-0003-3681-050X; Stroud, Rhonda/0000-0001-5242-8015; Burchell,
Mark/0000-0002-2680-8943
FU NASA [NNH11AQ61I, NNX09AC36G]; NASA Origins of Solar Systems Program;
Tawani Foundation; DFG [SPP1385]; Office of Science, Office of Basic
Energy Sciences, of the U.S. Department of Energy [DE-AC02-05CH11231];
U.S. Department of Energy, Office of Science, Office of Basic Energy
Sciences [DE-AC02-98CH10886]
FX We thank Fred Horz and Martin Lee for constructive reviews. RMS, HCG,
and NDB were supported by NASA grant NNH11AQ61I. JW. ALB, ZG, RL, DZ,
WM, and JVK were supported by NASA grant NNX09AC36G. SAS acknowledges
support from the NASA Origins of Solar Systems Program. PRH, AA, BH were
supported by the Tawani Foundation. PH and JL acknowledge support by DFG
through SPP1385: the first ten million years of the solar system-a
planetary materials approach. 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. Use of
the National Synchrotron Light Source, Brookhaven National Laboratory,
was supported by the U.S. Department of Energy, Office of Science,
Office of Basic Energy Sciences, under Contract No. DE-AC02-98CH10886.
NR 39
TC 9
Z9 9
U1 2
U2 15
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 1086-9379
EI 1945-5100
J9 METEORIT PLANET SCI
JI Meteorit. Planet. Sci.
PD SEP
PY 2014
VL 49
IS 9
SI SI
BP 1698
EP 1719
DI 10.1111/maps.12136
PG 22
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA AQ6HT
UT WOS:000342912100011
ER
PT J
AU Westphal, AJ
Bechtel, HA
Brenker, FE
Butterworth, AL
Flynn, G
Frank, DR
Gainsforth, Z
Hillier, JK
Postberg, F
Simionovici, AS
Sterken, VJ
Stroud, RM
Allen, C
Anderson, D
Ansari, A
Bajt, S
Bastien, RK
Bassim, N
Borg, J
Bridges, J
Brownlee, DE
Burchell, M
Burghammer, M
Changela, H
Cloetens, P
Davis, AM
Doll, R
Floss, C
Grun, E
Heck, PR
Hoppe, P
Hudson, B
Huth, J
Hvide, B
Kearsley, A
King, AJ
Lai, B
Leitner, J
Lemelle, L
Leroux, H
Leonard, A
Lettieri, R
Marchant, W
Nittler, LR
Ogliore, R
Ong, WJ
Price, MC
Sandford, SA
Tresseras, JAS
Schmitz, S
Schoonjans, T
Silversmit, G
Sole, VA
Srama, R
Stadermann, F
Stephan, T
Stodolna, J
Sutton, S
Trieloff, M
Tsou, P
Tsuchiyama, A
Tyliszczak, T
Vekemans, B
Vincze, L
Von Korff, J
Wordsworth, N
Zevin, D
Zolensky, ME
AF Westphal, Andrew J.
Bechtel, Hans A.
Brenker, Frank E.
Butterworth, Anna L.
Flynn, George
Frank, David R.
Gainsforth, Zack
Hillier, Jon K.
Postberg, Frank
Simionovici, Alexandre S.
Sterken, Veerle J.
Stroud, Rhonda M.
Allen, Carlton
Anderson, David
Ansari, Asna
Bajt, Sasa
Bastien, Ron K.
Bassim, Nabil
Borg, Janet
Bridges, John
Brownlee, Donald E.
Burchell, Mark
Burghammer, Manfred
Changela, Hitesh
Cloetens, Peter
Davis, Andrew M.
Doll, Ryan
Floss, Christine
Gruen, Eberhard
Heck, Philipp R.
Hoppe, Peter
Hudson, Bruce
Huth, Joachim
Hvide, Brit
Kearsley, Anton
King, Ashley J.
Lai, Barry
Leitner, Jan
Lemelle, Laurence
Leroux, Hugues
Leonard, Ariel
Lettieri, Robert
Marchant, William
Nittler, Larry R.
Ogliore, Ryan
Ong, Wei Ja
Price, Mark C.
Sandford, Scott A.
Tresseras, Juan-Angel Sans
Schmitz, Sylvia
Schoonjans, Tom
Silversmit, Geert
Sole, Vicente A.
Srama, Ralf
Stadermann, Frank
Stephan, Thomas
Stodolna, Julien
Sutton, Steven
Trieloff, Mario
Tsou, Peter
Tsuchiyama, Akira
Tyliszczak, Tolek
Vekemans, Bart
Vincze, Laszlo
Von Korff, Joshua
Wordsworth, Naomi
Zevin, Daniel
Zolensky, Michael E.
TI Final reports of the Stardust Interstellar Preliminary Examination
SO METEORITICS & PLANETARY SCIENCE
LA English
DT Article
ID ULYSSES DUST DATA
AB With the discovery of bona fide extraterrestrial materials in the Stardust Interstellar Dust Collector, NASA now has a fundamentally new returned sample collection, after the Apollo, Antarctic meteorite, Cosmic Dust, Genesis, Stardust Cometary, Hayabusa, and Exposed Space Hardware samples. Here, and in companion papers in this volume, we present the results from the Preliminary Examination of this collection, the Stardust Interstellar Preliminary Examination (ISPE). We found extraterrestrial materials in two tracks in aerogel whose trajectories and morphology are consistent with an origin in the interstellar dust stream, and in residues in four impacts in the aluminum foil collectors. While the preponderance of evidence, described in detail in companion papers in this volume, points toward an interstellar origin for some of these particles, alternative origins have not yet been eliminated, and definitive tests through isotopic analyses were not allowed under the terms of the ISPE. In this summary, we answer the central questions of the ISPE: How many tracks in the collector are consistent in their morphology and trajectory with interstellar particles? How many of these potential tracks are consistent with real interstellar particles, based on chemical analysis? Conversely, what fraction of candidates are consistent with either a secondary or interplanetary origin? What is the mass distribution of these particles, and what is their state? Are they particulate or diffuse? Is there any crystalline material? How many detectable impact craters (> 100 nm) are there in the foils, and what is their size distribution? How many of these craters have analyzable residue that is consistent with extraterrestrial material? And finally, can craters from secondaries be recognized through crater morphology (e.g., ellipticity)?
C1 [Westphal, Andrew J.; Butterworth, Anna L.; Gainsforth, Zack; Anderson, David; Lettieri, Robert; Marchant, William; Stodolna, Julien; Von Korff, Joshua; Zevin, Daniel] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
[Bechtel, Hans A.; Tyliszczak, Tolek] Lawrence Berkeley Lab, Adv Light Source, Berkeley, CA USA.
[Brenker, Frank E.; Schmitz, Sylvia] Goethe Univ Frankfurt, Inst Geosci, Frankfurt, Germany.
[Flynn, George] SUNY Coll Plattsburgh, Plattsburgh, NY 12901 USA.
[Frank, David R.; Bastien, Ron K.] NASA JSC, ESCG, Houston, TX USA.
[Hillier, Jon K.; Postberg, Frank; Trieloff, Mario] Heidelberg Univ, Inst Geowissensch, Heidelberg, Germany.
[Simionovici, Alexandre S.] Univ Grenoble, Observ Sci, Inst Sci Terre, Grenoble, France.
[Sterken, Veerle J.] Univ Stuttgart, IRS, D-70174 Stuttgart, Germany.
[Sterken, Veerle J.] Tech Univ Carolo Wilhelmina Braunschweig, IGEP, D-38106 Braunschweig, Germany.
[Sterken, Veerle J.; Zolensky, Michael E.] MPIK, Heidelberg, Germany.
[Stroud, Rhonda M.] Naval Res Lab, Mat Sci & Technol Div, Washington, DC USA.
[Allen, Carlton] NASA JSC, ARES, Houston, TX USA.
[Ansari, Asna; Hvide, Brit] Field Museum Nat Hist, Robert A Pritzker Ctr Meteorit & Polar Studies, Chicago, IL 60605 USA.
[Bajt, Sasa] DESY, Hamburg, Germany.
[Bassim, Nabil] Naval Res Lab, Nanoscale Mat Sect, Washington, DC USA.
[Borg, Janet] IAS Orsay, Orsay, France.
[Bridges, John] Univ Leicester, Space Res Ctr, Leicester, Leics, England.
[Brownlee, Donald E.] Univ Washington, Dept Astron, Seattle, WA 98195 USA.
[Burchell, Mark; Price, Mark C.] Univ Kent, Canterbury, Kent, England.
[Burghammer, Manfred; Cloetens, Peter; Tresseras, Juan-Angel Sans; Sole, Vicente A.] European Synchrotron Radiat Facil, F-38043 Grenoble, France.
[Changela, Hitesh] George Washington Univ, Washington, DC USA.
[Davis, Andrew M.; Stephan, Thomas] Univ Chicago, Chicago, IL 60637 USA.
[Doll, Ryan; Floss, Christine; Leonard, Ariel; Ong, Wei Ja; Stadermann, Frank] Washington Univ, St Louis, MO USA.
[Gruen, Eberhard] Max Planck Inst Kernphys, D-69117 Heidelberg, Germany.
[Heck, Philipp R.] Field Museum Nat Hist, Chicago, IL 60605 USA.
[Hoppe, Peter; Huth, Joachim; Leitner, Jan] Max Planck Inst Chem, D-55128 Mainz, Germany.
[Kearsley, Anton] Nat Hist Museum, London SW7 5BD, England.
[King, Ashley J.] Univ Chicago, Chicago, IL 60637 USA.
[King, Ashley J.] Field Museum Nat Hist, Robert A Pritzker Ctr Meteorit & Polar Studies, Chicago, IL 60605 USA.
[Lai, Barry; Sutton, Steven] Argonne Natl Lab, Adv Photon Source, Chicago, IL USA.
[Lemelle, Laurence] Ecole Normale Super Lyon, F-69364 Lyon, France.
[Leroux, Hugues] Univ Lille 1, Lille, France.
[Nittler, Larry R.] Carnegie Inst Sci, Washington, DC USA.
[Ogliore, Ryan] Univ Hawaii Manoa, Honolulu, HI 96822 USA.
[Sandford, Scott A.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Schoonjans, Tom; Silversmit, Geert; Vekemans, Bart; Vincze, Laszlo] Univ Ghent, B-9000 Ghent, Belgium.
[Srama, Ralf] Univ Stuttgart, IRS, D-70174 Stuttgart, Germany.
[Tsou, Peter] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Tsuchiyama, Akira] Osaka Univ, Osaka, Japan.
RP Westphal, AJ (reprint author), Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
EM westphal@ssl.berkeley.edu
RI Sans Tresserras, Juan Angel/J-9362-2014; Bajt, Sasa/G-2228-2010; Stroud,
Rhonda/C-5503-2008; Leitner, Jan/A-7391-2015; Hoppe, Peter/B-3032-2015
OI Sans Tresserras, Juan Angel/0000-0001-9047-3992; Stroud,
Rhonda/0000-0001-5242-8015; Burchell, Mark/0000-0002-2680-8943; Leitner,
Jan/0000-0003-3655-6273; Hoppe, Peter/0000-0003-3681-050X
NR 25
TC 12
Z9 12
U1 3
U2 20
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 1086-9379
EI 1945-5100
J9 METEORIT PLANET SCI
JI Meteorit. Planet. Sci.
PD SEP
PY 2014
VL 49
IS 9
SI SI
BP 1720
EP 1733
DI 10.1111/maps.12221
PG 14
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA AQ6HT
UT WOS:000342912100012
ER
PT J
AU Nichols, JE
Peteet, DM
Moy, CM
Castaneda, IS
McGeachy, A
Perez, M
AF Nichols, Jonathan E.
Peteet, Dorothy M.
Moy, Christopher M.
Castaneda, Isla S.
McGeachy, Alicia
Perez, Max
TI Impacts of climate and vegetation change on carbon accumulation in a
south-central Alaskan peatland assessed with novel organic geochemical
techniques
SO HOLOCENE
LA English
DT Article
DE carbon cycle; organic geochemistry; paleoclimate; paleoecology;
peatlands; stable isotopes
ID DELTA-D VALUES; DIALKYL GLYCEROL TETRAETHERS;
IONIZATION-MASS-SPECTROMETRY; N-ALKANES; METEORIC PRECIPITATION;
ISOTOPIC COMPOSITION; NORTHERN MINNESOTA; OMBROTROPHIC PEAT;
MEMBRANE-LIPIDS; WATER-CONTENT
AB To constrain the effect of climate and peatland type on carbon accumulation, we reconstructed these parameters from a Holocene-length core of a Sphagnum-dominated peatland near Cordova, AK, USA. We determined peat type using a combination of peat texture and density, macrofossils, distributions of leaf-wax biomarkers, and soil pH reconstructions based on distributions of branched glycerol dialkyl glycerol tetraether lipids (brGDGTs). We produced an independent record of hydroclimate and temperature change using hydrogen isotope ratios of leaf-wax biomarkers and distributions of brGDGTs. Carbon accumulation rates were constrained with 14 AMS C-14 dates from identified macrofossils and ash-free bulk density. In the early Holocene, the site was a shallow pond with evidence for emergent macrophytes, Sphagnum, and algae growing in a warm, moist climate. At 9.2 kyr (1 kyr = 1000 cal. yr BP), the site became a Sphagnum-dominated bog. Under mid-Holocene warm, evaporative climate conditions, the site became sedge-dominated. As climate cooled and effective precipitation increased, Sphagnum was able to gain dominance abruptly at similar to 3.5 kyr. Large changes in the vegetation assemblage and hydrology and climate are contemporaneous with significant changes in the rate of carbon accumulation. Carbon accumulated most rapidly when Sphagnum dominated and effective moisture was high and most slowly when sedges were dominant and conditions were warmer and drier. Estimates of future climate change indicate warmer, more evaporative conditions that, in the past, favored a sedge-dominated environment, suggesting that this peatland and those similar can contribute to a positive feedback to warming by transitioning to less efficient carbon sinks.
C1 [Nichols, Jonathan E.; Peteet, Dorothy M.] Lamont Doherty Earth Observ, Palisades, NY 10964 USA.
[Peteet, Dorothy M.] NASA, Goddard Inst Space Studies, Houston, TX USA.
[Moy, Christopher M.] Univ Otago, Dunedin, New Zealand.
[Castaneda, Isla S.] Univ Massachusetts, Amherst, MA 01003 USA.
[McGeachy, Alicia] Spelman Coll, Atlanta, GA USA.
[McGeachy, Alicia] Northwestern Univ, Evanston, IL 60208 USA.
[Perez, Max] SUNY Binghamton, Binghamton, NY 13902 USA.
RP Nichols, JE (reprint author), Lamont Doherty Earth Observ, 101D Paleomagnetics,61 Route 9W, Palisades, NY 10964 USA.
EM jnichols@ldeo.columbia.edu
FU US National Science Foundation [ARC-1022979]; Climate Center of the
Lamont-Doherty Earth Observatory; NASA Postdoctoral Program; US
Geological Survey Mendenhall Postdoctoral Fellowship
FX This work is supported by the US National Science Foundation ARC-1022979
and by the Climate Center of the Lamont-Doherty Earth Observatory. JEN
and CMM also gratefully acknowledge support from the NASA Postdoctoral
Program and the US Geological Survey Mendenhall Postdoctoral Fellowship,
respectively.
NR 52
TC 6
Z9 7
U1 3
U2 41
PU SAGE PUBLICATIONS LTD
PI LONDON
PA 1 OLIVERS YARD, 55 CITY ROAD, LONDON EC1Y 1SP, ENGLAND
SN 0959-6836
EI 1477-0911
J9 HOLOCENE
JI Holocene
PD SEP
PY 2014
VL 24
IS 9
SI SI
BP 1146
EP 1155
DI 10.1177/0959683614540729
PG 10
WC Geography, Physical; Geosciences, Multidisciplinary
SC Physical Geography; Geology
GA AQ1XO
UT WOS:000342578200012
ER
PT J
AU De Witt, JK
Edwards, WB
Scott-Pandorf, MM
Norcross, JR
Gernhardt, ML
AF De Witt, John K.
Edwards, W. Brent
Scott-Pandorf, Melissa M.
Norcross, Jason R.
Gernhardt, Michael L.
TI The preferred walk to run transition speed in actual lunar gravity
SO JOURNAL OF EXPERIMENTAL BIOLOGY
LA English
DT Article
DE Biomechanics; Locomotion; Preferred transition speed; Microgravity;
Froude number
ID DYNAMIC SIMILARITY HYPOTHESIS; REDUCED GRAVITY; HUMAN LOCOMOTION
AB Quantifying the preferred transition speed (PTS) from walking to running has provided insight into the underlying mechanics of locomotion. The dynamic similarity hypothesis suggests that the PTS should occur at the same Froude number across gravitational environments. In normal Earth gravity, the PTS occurs at a Froude number of 0.5 in adult humans, but previous reports found the PTS occurred at Froude numbers greater than 0.5 in simulated lunar gravity. Our purpose was to (1) determine the Froude number at the PTS in actual lunar gravity during parabolic flight and (2) compare it with the Froude number at the PTS in simulated lunar gravity during overhead suspension. We observed that Froude numbers at the PTS in actual lunar gravity (1.39 +/- 0.45) and simulated lunar gravity (1.11 +/- 0.26) were much greater than 0.5. Froude numbers at the PTS above 1.0 suggest that the use of the inverted pendulum model may not necessarily be valid in actual lunar gravity and that earlier findings in simulated reduced gravity are more accurate than previously thought.
C1 [De Witt, John K.; Scott-Pandorf, Melissa M.; Norcross, Jason R.] Wyle Sci Technol & Engn Grp, Houston, TX 77058 USA.
[Edwards, W. Brent] Univ Calgary, Calgary, AB T2N 1N4, Canada.
[Gernhardt, Michael L.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA.
RP De Witt, JK (reprint author), Wyle Sci Technol & Engn Grp, Houston, TX 77058 USA.
EM john.k.dewitt@nasa.gov
FU Human Health and Countermeasures Element of the National Aeronautics and
Space Administration's Human Research Program
FX This work was a directed study funded by the Human Health and
Countermeasures Element of the National Aeronautics and Space
Administration's Human Research Program.
NR 12
TC 6
Z9 6
U1 2
U2 9
PU COMPANY OF BIOLOGISTS LTD
PI CAMBRIDGE
PA BIDDER BUILDING CAMBRIDGE COMMERCIAL PARK COWLEY RD, CAMBRIDGE CB4 4DL,
CAMBS, ENGLAND
SN 0022-0949
EI 1477-9145
J9 J EXP BIOL
JI J. Exp. Biol.
PD SEP
PY 2014
VL 217
IS 18
BP 3200
EP 3203
DI 10.1242/jeb.105684
PG 4
WC Biology
SC Life Sciences & Biomedicine - Other Topics
GA AQ0XN
UT WOS:000342506100009
PM 25232195
ER
PT J
AU Lopez, RA
Moya, PS
Munoz, V
Vinas, AF
Valdivia, JA
AF Lopez, Rodrigo A.
Moya, Pablo S.
Munoz, Victor
Vinas, Adolfo F.
Alejandro Valdivia, J.
TI Kinetic transverse dispersion relation for relativistic magnetized
electron-positron plasmas with Maxwell-Juttner velocity distribution
functions
SO PHYSICS OF PLASMAS
LA English
DT Article
ID POLARIZED ELECTROMAGNETIC-WAVES; HOT ACCRETION DISKS; PARAMETRIC DECAYS
AB We use a kinetic treatment to study the linear transverse dispersion relation for a magnetized isotropic relativistic electron-positron plasma with finite relativistic temperature. The explicit linear dispersion relation for electromagnetic waves propagating along a constant background magnetic field is presented, including an analytical continuation to the whole complex frequency plane for the case of Maxwell-Juttner velocity distribution functions. This dispersion relation is studied numerically for various temperatures. For left-handed solutions, the system presents two branches, the electromagnetic ordinary mode and the Alfven mode. In the low frequency regime, the Alfven branch has two dispersive zones, the normal zone (where partial derivative omega/partial derivative k > 0) and an anomalous zone (where partial derivative x/partial derivative k < 0). We find that in the anomalous zone of the Alfven branch, the electromagnetic waves are damped, and there is a maximum wave number for which the Alfven branch is suppressed. We also study the dependence of the Alfven velocity and effective plasma frequency with the temperature. We complemented the analytical and numerical approaches with relativistic full particle simulations, which consistently agree with the analytical results. (C) 2014 AIP Publishing LLC.
C1 [Lopez, Rodrigo A.] Univ Concepcion, Dept Fis, Fac Ciencias Fis & Matemat, Concepcion, Chile.
[Moya, Pablo S.; Vinas, Adolfo F.] NASA, Goddard Space Flight Ctr, Heliophys Sci Div, Geospace Phys Lab, Greenbelt, MD 20771 USA.
[Moya, Pablo S.] Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA.
[Munoz, Victor; Alejandro Valdivia, J.] Univ Chile, Fac Ciencias, Dept Fis, Santiago, Chile.
[Alejandro Valdivia, J.] CEDENNA, Ctr Desarrollo Nanociencia & Nanotecnol, Santiago, Chile.
RP Lopez, RA (reprint author), Univ Concepcion, Dept Fis, Fac Ciencias Fis & Matemat, Concepcion, Chile.
RI Moya, Pablo/C-3163-2011; Lopez, Rodrigo/H-7576-2013; Valdivia,
Juan/A-3631-2008; Munoz, Victor/A-2255-2008
OI Moya, Pablo/0000-0002-9161-0888; Valdivia, Juan/0000-0003-3381-9904;
FU CONICyT through FONDECyT Grant [1110135, 1110729, 1121144, 3140142];
CONICyT-Becas Chile; CEDENNA; NASA-Wind/SWE project
FX The authors thank Roberto Navarro for useful discussions. Also, we thank
the support of CONICyT through FONDECyT Grant Nos. 1110135 and 1110729
(J.A.V.); No. 1121144 (V.M.) and Postdoctoral Grant No. 3140142.
(R.A.L.) We also thank the CONICyT-Becas Chile program by providing
financial support for postdoctoral fellow (P.S.M.). We also thank
financial support from CEDENNA. A.F.V. would like to thank the
NASA-Wind/SWE project for their support.
NR 30
TC 6
Z9 6
U1 0
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 1070-664X
EI 1089-7674
J9 PHYS PLASMAS
JI Phys. Plasmas
PD SEP
PY 2014
VL 21
IS 9
AR 092107
DI 10.1063/1.4894679
PG 10
WC Physics, Fluids & Plasmas
SC Physics
GA AQ4JC
UT WOS:000342760900014
ER
PT J
AU Navarro, RE
Araneda, J
Munoz, V
Moya, PS
F-Vinas, A
Valdivia, JA
AF Navarro, Roberto E.
Araneda, Jaime
Munoz, Victor
Moya, Pablo S.
F-Vinas, Adolfo
Valdivia, Juan A.
TI Theory of electromagnetic fluctuations for magnetized multi-species
plasmas
SO PHYSICS OF PLASMAS
LA English
DT Article
ID PROTON TEMPERATURE ANISOTROPY; QUASI-THERMAL FLUCTUATIONS; SOLAR-WIND;
VELOCITY DISTRIBUTIONS; SPACE PLASMAS; IONS; INSTABILITIES; CONSTRAINT;
STREAMS; 0.3-AU
AB Analysis of electromagnetic fluctuations in plasma provides relevant information about the plasma state and its macroscopic properties. In particular, the solar wind persistently sustains a small but detectable level of magnetic fluctuation power even near thermal equilibrium. These fluctuations may be related to spontaneous electromagnetic fluctuations arising from the discreteness of charged particles. Here, we derive general expressions for the plasma fluctuations in a multi-species plasma following arbitrary distribution functions. This formalism, which generalizes and includes previous works on the subject, is then applied to the generation of electromagnetic fluctuations propagating along a background magnetic field in a plasma of two proton populations described by drifting bi-Maxwellians. (C) 2014 AIP Publishing LLC.
C1 [Navarro, Roberto E.; Munoz, Victor; Valdivia, Juan A.] Univ Chile, Fac Ciencias, Dept Fis, Santiago, Chile.
[Araneda, Jaime] Univ Concepcion, Dept Fis, Concepcion 4070386, Chile.
[Moya, Pablo S.; F-Vinas, Adolfo] NASA, Goddard Space Flight Ctr, Heliophys Sci Div, Geospace Phys Lab, Greenbelt, MD 20771 USA.
[Moya, Pablo S.] Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA.
[Valdivia, Juan A.] CEIBA Complejidad, Ctr Estudios Interdisciplinarios Basicos & Aplica, Bogota, Colombia.
RP Navarro, RE (reprint author), Univ Chile, Fac Ciencias, Dept Fis, Casilla 653, Santiago, Chile.
EM roberto.navarro@ug.uchile.cl
RI Moya, Pablo/C-3163-2011; Valdivia, Juan/A-3631-2008; Navarro,
Roberto/F-7045-2014; Araneda, Jaime/J-9245-2015; Munoz,
Victor/A-2255-2008
OI Moya, Pablo/0000-0002-9161-0888; Valdivia, Juan/0000-0003-3381-9904;
Navarro, Roberto/0000-0003-0782-1904;
FU FONDECyT [1110135, 1110729, 1130273, 1121144, 1110880]; CONICYT-Becas
Chile; CONICyT [21100691]; CEDENNA; NASA's Wind/SWE program
FX This project has been financially supported by FONDECyT under contract
Nos. 1110135 (J.A.V.), 1110729 (J.A.V.), 1130273 (J.A.V.), 1121144 (V.
M.), and 1110880 (J.A). P.S.M thanks a Postdoctoral Fellowship from
CONICYT-Becas Chile. R.N. thanks a doctoral fellowship from CONICyT No.
21100691. J.A.V. also thanks to CEDENNA and A.F.V. thanks to NASA's
Wind/SWE program for their support.
NR 48
TC 11
Z9 11
U1 0
U2 2
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
EI 1089-7674
J9 PHYS PLASMAS
JI Phys. Plasmas
PD SEP
PY 2014
VL 21
IS 9
AR 092902
DI 10.1063/1.4894700
PG 7
WC Physics, Fluids & Plasmas
SC Physics
GA AQ4JC
UT WOS:000342760900069
ER
PT J
AU Govindarajan, N
de Visser, CC
Krishnakumar, K
AF Govindarajan, Nithin
de Visser, Cornelis. C.
Krishnakumar, Kalmanje
TI A sparse collocation method for solving time-dependent HJB equations
using multivariate B-splines
SO AUTOMATICA
LA English
DT Article
DE Optimal feedback control; Hamilton-Jacobi-Bellman equation; Adaptive
dynamic programming; Splines; Collocation method
ID JACOBI-BELLMAN EQUATIONS; NUMERICAL-SOLUTION; NONLINEAR-SYSTEMS
AB This paper presents a sparse collocation method for solving the time-dependent Hamilton-Jacobi-Bellman (HJB) equation associated with the continuous-time optimal control problem on a fixed, finite time-horizon with integral cost functional. Through casting the problem in a recursive framework using the value-iteration procedure, the value functions of every iteration step is approximated with a time-varying multivariate simplex B-spline on a certain state domain of interest. In the collocation scheme, the time-dependent coefficients of the spline function are further approximated with ordinary univariate B-splines to yield a discretization for the value function fully in terms of piece-wise polynomials. The B-spline coefficients are determined by solving a sequence of highly sparse quadratic programming problems. The proposed algorithm is demonstrated on a pair of benchmark example problems. Simulation results indicate that the method can yield increasingly more accurate approximations of the value function by refinement of the triangulation. (C) 2014 Elsevier Ltd. All rights reserved.
C1 [Govindarajan, Nithin] Delft Univ Technol, Fac Mech Maritime & Mat Engn, Delft Ctr Syst & Control, NL-2628 CD Delft, Netherlands.
[de Visser, Cornelis. C.] Delft Univ Technol, Fac Aerosp Engn, Control & Simulat Div, NL-2600 GB Delft, Netherlands.
[Krishnakumar, Kalmanje] NASA, Ames Res Ctr, Intelligent Syst Div, Moffett Field, CA 94035 USA.
RP Govindarajan, N (reprint author), Delft Univ Technol, Fac Mech Maritime & Mat Engn, Delft Ctr Syst & Control, NL-2628 CD Delft, Netherlands.
EM N.Govindarajan@student.tudelft.nl; C.C.deVisser@tudelft.nl;
k.krishnakumar@nasa.gov
NR 31
TC 1
Z9 1
U1 0
U2 13
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0005-1098
EI 1873-2836
J9 AUTOMATICA
JI Automatica
PD SEP
PY 2014
VL 50
IS 9
BP 2234
EP 2244
DI 10.1016/j.automatica.2014.07.012
PG 11
WC Automation & Control Systems; Engineering, Electrical & Electronic
SC Automation & Control Systems; Engineering
GA AQ0NG
UT WOS:000342479400003
ER
PT J
AU Lee, HH
Piner, KR
Hinton, MG
Chang, YJ
Kimoto, A
Kanaiwa, M
Su, NJ
Walsh, W
Sun, CL
DiNardo, G
AF Lee, Hui-Hua
Piner, Kevin R.
Hinton, Michael G.
Chang, Yi-Jay
Kimoto, Ai
Kanaiwa, Minoru
Su, Nan-Jay
Walsh, William
Sun, Chi-Lu
DiNardo, Gerard
TI Sex-structured population dynamics of blue marlin Makaira nigricans in
the Pacific Ocean
SO FISHERIES SCIENCE
LA English
DT Article
DE Sexual dimorphism; Sex structure; Age structure; Selectivity; Pacific
Ocean; Blue marlin
ID STOCK ASSESSMENT MODELS; ISTIOPHORID BILLFISHES; FISHERIES; GROWTH; AGE
AB The population dynamics of the blue marlin Makaira nigricans stock in the Pacific Ocean were estimated for 1971-2011 using a fully integrated length-based, age-, and sex-structured model. Fishery-specific catch, size composition, and catch-per-unit of effort were used in the modeling as likelihood components. Estimated dynamics were consistent with a stock that is fully exploited and stable over the last several years. No significant trends in recruitment were noted; however, female blue marlin were estimated to make up a majority of the catch, and historical exploitation has disproportionately changed the age structure of females relative to males. This result is due to differences in assumed life history and estimated selectivity. Changes to important life history parameters that are responsible for the productivity of the stock would potentially change the interpretation of current stock status.
C1 [Lee, Hui-Hua; Chang, Yi-Jay; Walsh, William] Univ Hawaii, Joint Inst Marine & Atmospher Res, Honolulu, HI 96818 USA.
[Piner, Kevin R.] NOAA, SW Fisheries Sci Ctr, Natl Marine Fisheries Serv, La Jolla, CA 92037 USA.
[Hinton, Michael G.] Interamer Trop Tuna Commiss, La Jolla, CA 92037 USA.
[Kimoto, Ai] Natl Res Inst Far Seas Fisheries, Shimizu, Shizuoka 4248633, Japan.
[Kanaiwa, Minoru] Tokyo Univ Agr, Abashiri, Hokkaido 0992493, Japan.
[Su, Nan-Jay; Sun, Chi-Lu] Natl Taiwan Univ, Inst Oceanog, Taipei 106, Taiwan.
[DiNardo, Gerard] NOAA, Pacific Isl Fisheries Sci Ctr, Natl Marine Fisheries Serv, Honolulu, HI 96818 USA.
RP Lee, HH (reprint author), Univ Hawaii, Joint Inst Marine & Atmospher Res, 1845 Wasp Blvd,Bldg 176, Honolulu, HI 96818 USA.
EM huihua.lee@noaa.gov; kevin.piner@noaa.gov; mhinton@iattc.org;
aikimoto@affrc.go.jp; m3kanaiw@bioindustry.nodai.ac.jp;
chilu@ntu.edu.tw; gerard.dinardo@noaa.gov
OI Chang, Yi-Jay/0000-0002-7472-4672
NR 26
TC 3
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U1 0
U2 8
PU SPRINGER JAPAN KK
PI TOKYO
PA CHIYODA FIRST BLDG EAST, 3-8-1 NISHI-KANDA, CHIYODA-KU, TOKYO, 101-0065,
JAPAN
SN 0919-9268
EI 1444-2906
J9 FISHERIES SCI
JI Fish. Sci.
PD SEP
PY 2014
VL 80
IS 5
BP 869
EP 878
DI 10.1007/s12562-014-0762-6
PG 10
WC Fisheries
SC Fisheries
GA AP6XC
UT WOS:000342220700001
ER
PT J
AU Kelsey, CR
Scott, J
Lane, A
Schwitzer, E
West, M
Thomas, S
Herndon, J
Michalski, M
Horwitz, M
Hennig, T
Jones, L
AF Kelsey, C. R.
Scott, J.
Lane, A.
Schwitzer, E.
West, M.
Thomas, S.
Herndon, J.
Michalski, M.
Horwitz, M.
Hennig, T.
Jones, L.
TI Cardiopulmonary Exercise Testing Prior to Myeloablative Allogeneic Stem
Cell Transplantation Using Total Body Irradiation: A Feasibility Study
SO INTERNATIONAL JOURNAL OF RADIATION ONCOLOGY BIOLOGY PHYSICS
LA English
DT Meeting Abstract
CT 56th Annual Meeting of the American-Society-for-Radiation-Oncology
CY SEP 14-17, 2014
CL San Francisco, CA
SP Amer Soc Radiat Oncol
C1 [Kelsey, C. R.; Lane, A.; Schwitzer, E.; West, M.; Thomas, S.; Herndon, J.; Michalski, M.; Horwitz, M.; Hennig, T.; Jones, L.] Duke Univ, Durham, NC USA.
[Scott, J.] NASA, Houston, TX USA.
NR 0
TC 0
Z9 0
U1 0
U2 0
PU ELSEVIER SCIENCE INC
PI NEW YORK
PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA
SN 0360-3016
EI 1879-355X
J9 INT J RADIAT ONCOL
JI Int. J. Radiat. Oncol. Biol. Phys.
PD SEP 1
PY 2014
VL 90
SU 1
MA 3195
BP S681
EP S681
PG 1
WC Oncology; Radiology, Nuclear Medicine & Medical Imaging
SC Oncology; Radiology, Nuclear Medicine & Medical Imaging
GA AP8LV
UT WOS:000342331402410
ER
PT J
AU Ditty, JG
AF Ditty, James G.
TI STERNAL SPINES IN PENAEID POSTLARVAE (DECAPODA: PENAEIDAE):
LIFE-PHASE-SPECIFIC AND SYSTEMATICALLY SIGNIFICANT?
SO JOURNAL OF CRUSTACEAN BIOLOGY
LA English
DT Article
DE developmental plasticity; Parapenaeus; penaeid diversity; sternal plate
shape; sternal spine patterns
ID SHRIMP FARFANTEPENAEUS-DUORARUM; EARLY DEVELOPMENTAL-STAGES;
INDIAN-OCEAN EXPEDITION; INDO-WEST PACIFIC; GULF-OF-MEXICO; LARVAL
DEVELOPMENT; GENUS PENAEUS; CRUSTACEA DECAPODA; RATHBUN DECAPODA;
TAXONOMIC VALUE
AB Our ability to identify and discriminate postlarvae of penaeids below family level remains poor due to phase brevity and a lack of taxonomic characters. Whether sternal spines are unique and taxonomically significant to postlarvae has not been resolved. I describe number and placement of spines in Parapenaeus sp. Smith, 1885, and a specimen tentatively identified as Xiphopenaeus kroyeri (Heller, 1862) from the Gulf of Mexico; review information for penaeids worldwide; and evaluate the significance of sternal spines as a life-phase specific taxonomic character and to penaeid systematics. To date, sternal spines have been described for 14 of 32 genera and 26 species. Most taxa share one of two common sternal formulas: either 0 + 0 + 0 + 1 + 0, or 0 + 0 + 0 + 1 + 1. Only Metapenaeopsis Bouvier, 1905, and the tentative Xiphopenaeus kroyeri have a pair of spines on at least the first-two sternal plates, and only Metapenaeopsis and Litopenaeus Perez-Farfante, 1969, contain members with different sternal formulas. I suggest that differences among taxa in shape of the sternal plates may be an unrecognized taxonomic character. Sternal spines are not life-phase specific and do not reflect lower-level systematic relationships within Penaeidae regardless of generic nomenclature applied. The unusual length, shape, and reverse orientation of the spine on plate five in species of Parapenaeus, and presence of an elongate ventromedian spine on one or more pleomeres in Parapenaeus and Funchalia Johnson, 1868, supports molecular and morphological data that Penaeidae may be paraphyletic. While generally ineffective as a stand-alone taxonomic character, differences in number, placement, and orientation of sternal spines, i.e., the 'sternal pattern'; knowledge of geographic distributions; and, perhaps differences in sternal plate shape should be included in the suite of characters used to discriminate and identify penaeids during the postlarva phase.
C1 Natl Marine Fisheries Serv, Natl Oceanog & Atmospher Adm, Galveston, TX 77551 USA.
RP Ditty, JG (reprint author), Natl Marine Fisheries Serv, Natl Oceanog & Atmospher Adm, 4700 Ave U, Galveston, TX 77551 USA.
EM Jim.Ditty@NOAA.gov
FU NOAA's Southeast Fisheries Science Center
FX Thanks to Dr. Antonina dos Santos, Instituto Portugues do Mar e da
Atmosfera, Lisbon, Portugal, for providing a postlarva of Melicertus
kerathurus collected off Portugal, and to Carley Knight, University of
Southern Mississippi and NOAA's Pascagoula Laboratory for myses and
postlarvae of Parapenaeus sp. from the Gulf of Mexico. Thanks to Dr.
Geoffrey Matthews (retired), formerly of NOAA's Galveston Laboratory,
and to Shawn Hillen and Juan Salas of NOAA's Galveston Laboratory who
participated in sample collection, and to NOAA's Southeast Fisheries
Science Center for funding support Thanks also to Juan Salas for
illustrating the sternal pattern for Litopenaeus setiferus,
Fatfantepenaeus aztecus, Melicertus kerathurus, Parapenaeus sp. and
tentative Xiphopenaeus kroyeri. Images were reproduced by kind
permission of the publishers through Rightslink (R): CSIRO Publishing
(Marine and Freshwater Research); Oxford University Press (Journal of
Plankton Research); Springer (Hydrobiologia) with permission from
Springer Science + Business Media; and courtesy of NOAA Fisheries
(Fishery Bulletin). Views and opinions expressed here are those of the
author and do not necessarily reflect those of NOAA Fisheries.
NR 120
TC 0
Z9 0
U1 1
U2 8
PU CRUSTACEAN SOC
PI SAN ANTONIO
PA 840 EAST MULBERRY, SAN ANTONIO, TX 78212 USA
SN 0278-0372
EI 1937-240X
J9 J CRUSTACEAN BIOL
JI J. Crustac. Biol.
PD SEP
PY 2014
VL 34
IS 5
BP 618
EP 628
DI 10.1163/1937240X-00002261
PG 11
WC Marine & Freshwater Biology
SC Marine & Freshwater Biology
GA AP9IH
UT WOS:000342393000010
ER
PT J
AU Carpenter, JR
Markley, FL
AF Carpenter, J. Russell
Markley, F. Landis
TI Wald Sequential Probability Ratio Test for Space Object Conjunction
Assessment
SO JOURNAL OF GUIDANCE CONTROL AND DYNAMICS
LA English
DT Article
ID SATELLITE COLLISION PROBABILITY; AVOIDANCE MANEUVER DECISIONS; ORBIT
UNCERTAINTY; TERM ENCOUNTERS; PROPAGATION; RISK
AB This paper shows how satellite owners/operators may use sequential estimates of collision probability, along with a prior assessment of the base risk of collision, in a compound hypothesis ratio test to inform decisions concerning collision risk mitigation maneuvers. The compound hypothesis test reduces to a simple probability ratio test, which appears to be a novel result. The test satisfies tolerances related to targeted false alarm and missed detection rates. This result is independent of the method one uses to compute the probability density that one integrates to compute collision probability. A well-established test case from the literature shows that this test yields acceptable results within the constraints of a typical operational conjunction assessment decision timeline. Another example illustrates the use of the test in a practical conjunction assessment scenario based on operations of the International Space Station.
C1 [Carpenter, J. Russell] NASA, Goddard Space Flight Ctr, Nav & Mission Design Branch, Greenbelt, MD 20771 USA.
[Markley, F. Landis] NASA, Goddard Space Flight Ctr, Attitude Control Syst Engn Branch, Greenbelt, MD 20771 USA.
RP Carpenter, JR (reprint author), NASA, Goddard Space Flight Ctr, Nav & Mission Design Branch, Code 595, Greenbelt, MD 20771 USA.
NR 33
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 0731-5090
EI 1533-3884
J9 J GUID CONTROL DYNAM
JI J. Guid. Control Dyn.
PD SEP-OCT
PY 2014
VL 37
IS 5
BP 1385
EP 1396
DI 10.2514/1.G000478
PG 12
WC Engineering, Aerospace; Instruments & Instrumentation
SC Engineering; Instruments & Instrumentation
GA AP7FS
UT WOS:000342243800001
ER
PT J
AU Heath, CM
AF Heath, Christopher M.
TI Characterization of Swirl-Venturi Lean Direct Injection Designs for
Aviation Gas Turbine Combustion
SO JOURNAL OF PROPULSION AND POWER
LA English
DT Article
AB Injector geometry, physical mixing, chemical processes, and engine cycle conditions together govern performance, operability, and emission characteristics of aviation gas turbine combustion systems. The present investigation explores swirl-venturi lean direct injection combustor fundamentals, characterizing the influence of key geometric injector parameters on reacting flow physics and emission production trends. In this computational study, a design space exploration was performed using a parameterized swirl-venturi lean direct injector model. From the parametric geometry, 20 three-element lean direct injection combustor sectors were produced and simulated using steady-state Reynolds-averaged Navier-Stokes reacting computations. Species concentrations were solved directly using a reduced 18-step reaction mechanism for Jet A. Turbulence closure was obtained using a nonlinear kappa-epsilon model. Results demonstrate sensitivities of the geometric perturbations on axially averaged flowfield responses. Output variables include axial velocity, turbulent kinetic energy, static temperature, fuel patternation, and minor species mass fractions. Significant trends have been reduced to surrogate model approximations, intended to guide future injector design trade studies and advance aviation gas turbine combustion research.
C1 NASA, John H Glenn Res Ctr Lewis Field, Multidisciplinary Design Anal & Optimizat Branch, Cleveland, OH 44135 USA.
RP Heath, CM (reprint author), NASA, John H Glenn Res Ctr Lewis Field, Multidisciplinary Design Anal & Optimizat Branch, MS 5-10, Cleveland, OH 44135 USA.
FU Supersonics and Fixed Wing Projects of the NASA Fundamental Aeronautics
Program
FX The author gratefully acknowledges the support of the Supersonics and
Fixed Wing Projects of the NASA Fundamental Aeronautics Program. Also, a
special thanks to Jonathan Seidel for providing the inspiration for this
research; Jeffrey Moder for the numerous enhancements made to the
National Combustion Code; and the NASA OpenMDAO development team,
especially Justin Gray, for providing software integration assistance.
NR 30
TC 1
Z9 1
U1 3
U2 13
PU AMER INST AERONAUTICS ASTRONAUTICS
PI RESTON
PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA
SN 0748-4658
EI 1533-3876
J9 J PROPUL POWER
JI J. Propul. Power
PD SEP-OCT
PY 2014
VL 30
IS 5
BP 1334
EP 1356
DI 10.2514/1.B35077
PG 23
WC Engineering, Aerospace
SC Engineering
GA AQ1HG
UT WOS:000342531900021
ER
PT J
AU Agee, CB
Muttik, N
Ziegler, K
Walton, EL
Herd, CDK
McCubbin, FM
Santos, AR
Burger, PV
Simon, JI
Peters, TJ
Tappa, MJ
Sanborn, ME
Yin, QZ
AF Agee, C. B.
Muttik, N.
Ziegler, K.
Walton, E. L.
Herd, C. D. K.
McCubbin, F. M.
Santos, A. R.
Burger, P. V.
Simon, J. I.
Peters, T. J.
Tappa, M. J.
Sanborn, M. E.
Yin, Q-Z.
TI NEW METEORITE TYPE NWA 8159 AUGITE BASALT: SPECIMEN FROM A PREVIOUSLY
UNSAMPLED LOCATION ON MARS?
SO METEORITICS & PLANETARY SCIENCE
LA English
DT Meeting Abstract
CT 77th Annual Meeting of the Meteoritical-Society
CY SEP 08-13, 2014
CL Casablanca, MOROCCO
SP Meteorit Soc
C1 [Agee, C. B.; Muttik, N.; Ziegler, K.; McCubbin, F. M.; Santos, A. R.; Burger, P. V.] Univ New Mexico, Inst Meteorit, Albuquerque, NM 87131 USA.
[Agee, C. B.; Muttik, N.; Ziegler, K.; McCubbin, F. M.; Santos, A. R.; Burger, P. V.] Univ New Mexico, Dept Earth & Planetary Sci, Albuquerque, NM 87131 USA.
[Walton, E. L.; Herd, C. D. K.] Univ Alberta, Dept Earth & Atmospher Sci, Edmonton, AB T6G 2M7, Canada.
[Simon, J. I.; Peters, T. J.; Tappa, M. J.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA.
[Peters, T. J.] LPI, Houston, TX USA.
[Tappa, M. J.] JETS Jacobs Technol, Houston, TX USA.
[Sanborn, M. E.; Yin, Q-Z.] Univ Calif Davis, Dept Earth & Planetary Sci, Sacramento, CA USA.
NR 2
TC 0
Z9 0
U1 0
U2 0
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 1086-9379
EI 1945-5100
J9 METEORIT PLANET SCI
JI Meteorit. Planet. Sci.
PD SEP
PY 2014
VL 49
SU 1
SI SI
BP A11
EP A11
PG 1
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA AP2PA
UT WOS:000341914200008
ER
PT J
AU Bishop, JL
Tirsch, D
AF Bishop, J. L.
Tirsch, D.
TI VNIR SPECTRAL PROPERTIES OF MARTIAN METEORITES AND COMPARISON WITH CRISM
SPECTRA OF MARS IN THE ISIDIS BASIN REGION
SO METEORITICS & PLANETARY SCIENCE
LA English
DT Meeting Abstract
CT 77th Annual Meeting of the Meteoritical-Society
CY SEP 08-13, 2014
CL Casablanca, MOROCCO
SP Meteorit Soc
C1 [Bishop, J. L.] SETI Inst, Carl Sagan Ctr, Mountain View, CA USA.
[Bishop, J. L.] NASA Ames, Mountain View, CA USA.
[Tirsch, D.] German Aerosp Ctr DLR, Inst Planetary Res, Berlin, Germany.
EM jbishop@seti.org
NR 4
TC 0
Z9 0
U1 0
U2 0
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 1086-9379
EI 1945-5100
J9 METEORIT PLANET SCI
JI Meteorit. Planet. Sci.
PD SEP
PY 2014
VL 49
SU 1
SI SI
BP A42
EP A42
PG 1
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA AP2PA
UT WOS:000341914200039
ER
PT J
AU Blumenfeld, EH
Evans, CA
Oshel, ER
Liddle, DA
Beaulieu, K
Zeigler, RA
Righter, K
Hanna, RD
Ketcham, RA
AF Blumenfeld, E. H.
Evans, C. A.
Oshel, E. R.
Liddle, D. A.
Beaulieu, K.
Zeigler, R. A.
Righter, K.
Hanna, R. D.
Ketcham, R. A.
TI High-Resolution Imaged-Based 3D Reconstruction Combined with X-Ray CT
Data Enables Comprehensive Non-Destructive Documentation and Targeted
Research of Astromaterials
SO METEORITICS & PLANETARY SCIENCE
LA English
DT Meeting Abstract
CT 77th Annual Meeting of the Meteoritical-Society
CY SEP 08-13, 2014
CL Casablanca, MOROCCO
SP Meteorit Soc
C1 [Blumenfeld, E. H.] Hamad bin Khalifa Univ, UCL Qatar, Doha, Qatar.
[Evans, C. A.; Zeigler, R. A.; Righter, K.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA.
[Oshel, E. R.; Liddle, D. A.; Beaulieu, K.] NASA, Lyndon B Johnson Space Ctr, JETS, Houston, TX 77058 USA.
[Hanna, R. D.; Ketcham, R. A.] Univ Texas Austin, Jackson Sch Geosci, UTCT Facil, Austin, TX 78712 USA.
EM e.blumenfeld.12@ucl.ac.uk
RI Ketcham, Richard/B-5431-2011
OI Ketcham, Richard/0000-0002-2748-0409
NR 3
TC 0
Z9 0
U1 1
U2 1
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 1086-9379
EI 1945-5100
J9 METEORIT PLANET SCI
JI Meteorit. Planet. Sci.
PD SEP
PY 2014
VL 49
SU 1
SI SI
BP A46
EP A46
PG 1
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA AP2PA
UT WOS:000341914200043
ER
PT J
AU Bottke, WF
Swindle, TD
Marchi, S
Scott, ERD
Vokrouhlicky, D
Weirich, JR
AF Bottke, W. F.
Swindle, T. D.
Marchi, S.
Scott, E. R. D.
Vokrouhlicky, D.
Weirich, J. R.
TI USING METEORITES TO FIND THE AGE OF THE MOON-FORMING EVENT
SO METEORITICS & PLANETARY SCIENCE
LA English
DT Meeting Abstract
CT 77th Annual Meeting of the Meteoritical-Society
CY SEP 08-13, 2014
CL Casablanca, MOROCCO
SP Meteorit Soc
ID GIANT IMPACT; EARTH
C1 [Bottke, W. F.; Marchi, S.] SW Res Inst, Boulder, CO USA.
[Bottke, W. F.; Swindle, T. D.; Marchi, S.] NASA, SSERVI, Washington, DC USA.
[Swindle, T. D.] Univ Arizona, Tucson, AZ USA.
[Scott, E. R. D.] Univ Hawaii, Honolulu, HI 96822 USA.
[Vokrouhlicky, D.] Charles Univ Prague, Prague, Czech Republic.
[Weirich, J. R.] Univ Western Ontario, London, ON, Canada.
EM bottke@boulder.swri.edu
NR 7
TC 0
Z9 0
U1 0
U2 2
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 1086-9379
EI 1945-5100
J9 METEORIT PLANET SCI
JI Meteorit. Planet. Sci.
PD SEP
PY 2014
VL 49
SU 1
SI SI
BP A52
EP A52
PG 1
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA AP2PA
UT WOS:000341914200049
ER
PT J
AU Bridges, JC
Schwenzer, SP
Leveille, R
Westall, F
Wiens, RC
Mangold, N
Bristow, T
Edwards, P
Berger, G
AF Bridges, J. C.
Schwenzer, S. P.
Leveille, R.
Westall, F.
Wiens, R. C.
Mangold, N.
Bristow, T.
Edwards, P.
Berger, G.
TI CLAY AND MAGNETITE FORMATION AT YELLOWKNIFE BAY, MARS.
SO METEORITICS & PLANETARY SCIENCE
LA English
DT Meeting Abstract
CT 77th Annual Meeting of the Meteoritical-Society
CY SEP 08-13, 2014
CL Casablanca, MOROCCO
SP Meteorit Soc
C1 [Bridges, J. C.; Edwards, P.] Univ Leicester, Space Res Ctr, Leicester LE1 7RH, Leics, England.
[Schwenzer, S. P.] Open Univ, Milton Keynes MK7 6AA, Bucks, England.
[Leveille, R.] McGill Univ, Montreal, PQ, Canada.
[Westall, F.] CNRS, Ctr Biophys Mol, F-45071 Orleans, France.
[Wiens, R. C.] Los Alamos Natl Lab, Los Alamos, NM 87544 USA.
[Mangold, N.] Lab Planetol & Geodynam Nantes, Nantes, France.
[Mangold, N.] Univ Nantes, F-44035 Nantes, France.
[Bristow, T.] NASA, Ames Res Ctr, Exobiol Branch, Moffett Field, CA 94035 USA.
[Berger, G.] IRAP Obs Midi Pyrenees, Toulouse, France.
EM j.bridges@le.ac.uk
RI BERGER, Gilles/F-7118-2016
NR 8
TC 0
Z9 0
U1 0
U2 6
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 1086-9379
EI 1945-5100
J9 METEORIT PLANET SCI
JI Meteorit. Planet. Sci.
PD SEP
PY 2014
VL 49
SU 1
SI SI
BP A59
EP A59
PG 1
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA AP2PA
UT WOS:000341914200056
ER
PT J
AU Chennaoui-Aoudjehane, H
Larouci, N
Jambon, A
Mittlefehldt, DW
AF Chennaoui-Aoudjehane, H.
Larouci, N.
Jambon, A.
Mittlefehldt, D. W.
TI A CLASSIFICATION TABLE FOR ACHONDRITES (2)
SO METEORITICS & PLANETARY SCIENCE
LA English
DT Meeting Abstract
CT 77th Annual Meeting of the Meteoritical-Society
CY SEP 08-13, 2014
CL Casablanca, MOROCCO
SP Meteorit Soc
C1 [Chennaoui-Aoudjehane, H.; Larouci, N.] Hassan II Univ Casablanca, Fac Sci, Casablanca, Morocco.
[Jambon, A.] Univ Paris 06, ISTEP, F-75252 Paris, France.
[Mittlefehldt, D. W.] NASA, Astromat Res Off, Johnson Space Ctr, Houston, TX USA.
EM chennaoui_h@yahoo.fr
NR 6
TC 0
Z9 0
U1 0
U2 2
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 1086-9379
EI 1945-5100
J9 METEORIT PLANET SCI
JI Meteorit. Planet. Sci.
PD SEP
PY 2014
VL 49
SU 1
SI SI
BP A73
EP A73
PG 1
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA AP2PA
UT WOS:000341914200070
ER
PT J
AU Clemett, SJ
Nakamura-Messenger, K
Messenger, S
AF Clemett, S. J.
Nakamura-Messenger, K.
Messenger, S.
TI MASS SPECTUM IMAGING OF ORGANICS INJECTED INTO STARDUST AEROGEL BY
COMETARY IMPACTS.
SO METEORITICS & PLANETARY SCIENCE
LA English
DT Meeting Abstract
CT 77th Annual Meeting of the Meteoritical-Society
CY SEP 08-13, 2014
CL Casablanca, MOROCCO
SP Meteorit Soc
C1 [Clemett, S. J.] ERC Inc JACOBS, Houston, TX 77023 USA.
[Nakamura-Messenger, K.; Messenger, S.] NASA, A Robert M Walker Lab Space Sci, Johnson Space Ctr, Houston, TX 77058 USA.
EM simon.j.clemett@nasa.gov
NR 9
TC 0
Z9 0
U1 1
U2 2
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 1086-9379
EI 1945-5100
J9 METEORIT PLANET SCI
JI Meteorit. Planet. Sci.
PD SEP
PY 2014
VL 49
SU 1
SI SI
BP A76
EP A76
PG 1
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA AP2PA
UT WOS:000341914200073
ER
PT J
AU Day, JMD
Corder, CA
Dhaliwal, JK
Liu, Y
Taylor, LA
AF Day, J. M. D.
Corder, C. A.
Dhaliwal, J. K.
Liu, Y.
Taylor, L. A.
TI The Chelyabinsk fall highly siderophile element abundance and
Os-187/Os-188 composition and comparison with ordinary and carbonaceous
chondrites
SO METEORITICS & PLANETARY SCIENCE
LA English
DT Meeting Abstract
CT 77th Annual Meeting of the Meteoritical-Society
CY SEP 08-13, 2014
CL Casablanca, MOROCCO
SP Meteorit Soc
C1 [Day, J. M. D.; Corder, C. A.; Dhaliwal, J. K.] Univ Calif San Diego, Scripps Inst Oceanog, La Jolla, CA 92093 USA.
[Liu, Y.] CALTECH, JPL, Pasadena, CA 91109 USA.
[Taylor, L. A.] Univ Tennessee, Plametary Geosci Inst, Knoxville, TN 37996 USA.
EM jmdday@ucsd.edu
NR 6
TC 0
Z9 0
U1 0
U2 4
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 1086-9379
EI 1945-5100
J9 METEORIT PLANET SCI
JI Meteorit. Planet. Sci.
PD SEP
PY 2014
VL 49
SU 1
SI SI
BP A91
EP A91
PG 1
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA AP2PA
UT WOS:000341914200088
ER
PT J
AU Englert, P
Bishop, JL
Gibson, EK
Patel, S
Koeberl, C
AF Englert, P.
Bishop, J. L.
Gibson, E. K.
Patel, S.
Koeberl, C.
TI DON JUAN BASIN, WRIGHT VALLEY, ANTARCTICA: MODEL FOR SURFACE PROCESSES
ON MARS.
SO METEORITICS & PLANETARY SCIENCE
LA English
DT Meeting Abstract
CT 77th Annual Meeting of the Meteoritical-Society
CY SEP 08-13, 2014
CL Casablanca, MOROCCO
SP Meteorit Soc
C1 [Englert, P.] Univ Hawaii Manoa, Honolulu, HI 96822 USA.
[Bishop, J. L.; Patel, S.] SETI Inst, Mountain View, CA USA.
[Bishop, J. L.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Gibson, E. K.] Johnson Space Flight Ctr, Houston, TX USA.
[Patel, S.] San Jose State Univ, San Jose, CA 95192 USA.
[Koeberl, C.] Univ Vienna, Vienna, Austria.
EM penglert@hawaii.edu
NR 6
TC 0
Z9 0
U1 0
U2 0
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 1086-9379
EI 1945-5100
J9 METEORIT PLANET SCI
JI Meteorit. Planet. Sci.
PD SEP
PY 2014
VL 49
SU 1
SI SI
BP A110
EP A110
PG 1
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA AP2PA
UT WOS:000341914200107
ER
PT J
AU Fries, M
Steele, A
AF Fries, M.
Steele, A.
TI TOWARDS A GENERAL EQUATION FOR THE SURVIVAL OF MICROBES TRANSFERRED
BETWEEN SOLAR SYSTEM BODIES.
SO METEORITICS & PLANETARY SCIENCE
LA English
DT Meeting Abstract
CT 77th Annual Meeting of the Meteoritical-Society
CY SEP 08-13, 2014
CL Casablanca, MOROCCO
SP Meteorit Soc
C1 [Fries, M.] NASA, ARES, Johnson Space Ctr, Houston, TX USA.
[Steele, A.] Carnegie Inst Sci, Geophys Lab, Washington, DC 20015 USA.
EM marc.d.fries@nasa.gov
NR 4
TC 0
Z9 0
U1 0
U2 0
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 1086-9379
EI 1945-5100
J9 METEORIT PLANET SCI
JI Meteorit. Planet. Sci.
PD SEP
PY 2014
VL 49
SU 1
SI SI
BP A123
EP A123
PG 1
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA AP2PA
UT WOS:000341914200120
ER
PT J
AU Fries, M
Matson, R
Schaefer, J
Fries, J
Hankey, M
Anderson, L
AF Fries, Marc
Matson, Robert
Schaefer, Jacob
Fries, Jeffrey
Hankey, Mike
Anderson, Lindsay
TI WORLDWIDE WEATHER RADAR IMAGERY MAY ALLOW SUBSTANTIAL INCREASE IN
METEORITE FALL RECOVERY.
SO METEORITICS & PLANETARY SCIENCE
LA English
DT Meeting Abstract
CT 77th Annual Meeting of the Meteoritical-Society
CY SEP 08-13, 2014
CL Casablanca, MOROCCO
SP Meteorit Soc
C1 [Fries, Marc] NASA, ARES, Johnson Space Ctr, Houston, TX USA.
[Matson, Robert] Leidos Inc, Reston, VA 20190 USA.
[Fries, Jeffrey] USAF Weather Agcy, Weather Grp 1, Offutt AFB, NE 68113 USA.
[Hankey, Mike] Amer Meteor Soc, Geneseo, NY 14454 USA.
[Anderson, Lindsay] Univ N Dakota, Dept Space Studies, Grand Forks, ND 58202 USA.
EM marc.d.fries@nasa.gov
NR 3
TC 0
Z9 0
U1 0
U2 0
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 1086-9379
EI 1945-5100
J9 METEORIT PLANET SCI
JI Meteorit. Planet. Sci.
PD SEP
PY 2014
VL 49
SU 1
SI SI
BP A124
EP A124
PG 1
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA AP2PA
UT WOS:000341914200121
ER
PT J
AU Hallis, LJ
Huss, GR
Nagashima, K
Taylor, GJ
Stoffler, D
Smith, CL
Lee, MR
AF Hallis, L. J.
Huss, G. R.
Nagashima, K.
Taylor, G. J.
Stoeffler, D.
Smith, C. L.
Lee, M. R.
TI D/H AND WATER SOURCES IN TISSINT.
SO METEORITICS & PLANETARY SCIENCE
LA English
DT Meeting Abstract
CT 77th Annual Meeting of the Meteoritical-Society
CY SEP 08-13, 2014
CL Casablanca, MOROCCO
SP Meteorit Soc
C1 [Hallis, L. J.; Huss, G. R.; Taylor, G. J.] Univ Hawaii, NASA, Astrobiol Inst, Honolulu, HI 96822 USA.
[Hallis, L. J.; Huss, G. R.; Nagashima, K.; Taylor, G. J.] Univ Hawaii, Hawaii Inst Geophys & Planetol, Honolulu, HI 96822 USA.
[Stoeffler, D.] Museum Nat Hist, Berlin, Germany.
[Smith, C. L.] Nat Hist Museum, London, England.
[Hallis, L. J.; Lee, M. R.] Univ Glasgow, Sch Geog & Earth Sci, Glasgow G12 8QQ, Lanark, Scotland.
EM Lyd-ia.Hallis@glasgow.ac.uk
NR 9
TC 0
Z9 0
U1 0
U2 0
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 1086-9379
EI 1945-5100
J9 METEORIT PLANET SCI
JI Meteorit. Planet. Sci.
PD SEP
PY 2014
VL 49
SU 1
SI SI
BP A153
EP A153
PG 1
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA AP2PA
UT WOS:000341914200150
ER
PT J
AU Han, JM
Brearley, AJ
Keller, LP
AF Han, Jangmi
Brearley, Adrian J.
Keller, Lindsay P.
TI MICROSTRUCTURES OF HIBONITE FROM AN ALH A77307 (CO3.0) CAI: EVIDENCE FOR
EVAPORATIVE LOSS OF CALCIUM.
SO METEORITICS & PLANETARY SCIENCE
LA English
DT Meeting Abstract
CT 77th Annual Meeting of the Meteoritical-Society
CY SEP 08-13, 2014
CL Casablanca, MOROCCO
SP Meteorit Soc
ID METEORITES
C1 [Han, Jangmi] LPI, Houston, TX 77058 USA.
[Han, Jangmi; Keller, Lindsay P.] NASA, JSC, ARES, Robert M Walker Lab Space Sci, Houston, TX 77058 USA.
[Brearley, Adrian J.] Univ New Mexico, Dept Earth & Planetary Sci, Albuquerque, NM 87131 USA.
EM jangmi.han@nasa.gov
NR 6
TC 0
Z9 0
U1 0
U2 0
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 1086-9379
EI 1945-5100
J9 METEORIT PLANET SCI
JI Meteorit. Planet. Sci.
PD SEP
PY 2014
VL 49
SU 1
SI SI
BP A155
EP A155
PG 1
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA AP2PA
UT WOS:000341914200152
ER
PT J
AU Hanna, RD
Zolensky, M
Ketcham, RA
Behr, WM
Martinez, JE
AF Hanna, R. D.
Zolensky, M.
Ketcham, R. A.
Behr, W. M.
Martinez, J. E.
TI IMPACT-INDUCED CHONDRULE DEFORMATION AND AQUEOUS ALTERATION OF CM2
MURCHISON
SO METEORITICS & PLANETARY SCIENCE
LA English
DT Meeting Abstract
CT 77th Annual Meeting of the Meteoritical-Society
CY SEP 08-13, 2014
CL Casablanca, MOROCCO
SP Meteorit Soc
ID CARBONACEOUS CHONDRITES
C1 [Hanna, R. D.; Ketcham, R. A.; Behr, W. M.] Univ Texas Austin, Jackson Sch Geosci, Austin, TX 78712 USA.
[Zolensky, M.] NASA, ARES, Johnson Space Ctr, Houston, TX 77058 USA.
[Martinez, J. E.] NASA, Jacobs Technol, Johnson Space Ctr, Houston, TX 77058 USA.
EM romy@jsg.utexas.edu
RI Ketcham, Richard/B-5431-2011
OI Ketcham, Richard/0000-0002-2748-0409
NR 8
TC 0
Z9 0
U1 0
U2 0
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 1086-9379
EI 1945-5100
J9 METEORIT PLANET SCI
JI Meteorit. Planet. Sci.
PD SEP
PY 2014
VL 49
SU 1
SI SI
BP A156
EP A156
PG 1
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA AP2PA
UT WOS:000341914200153
ER
PT J
AU Hermalyn, B
AF Hermalyn, B.
TI EJECTA FROM TARGETS STRONG AND WEAK: EXPERIMENTAL MEASUREMENTS OF
STRENGTH CONTROLLED AND STRENGTHLESS CRATERS
SO METEORITICS & PLANETARY SCIENCE
LA English
DT Meeting Abstract
CT 77th Annual Meeting of the Meteoritical-Society
CY SEP 08-13, 2014
CL Casablanca, MOROCCO
SP Meteorit Soc
C1 [Hermalyn, B.] Univ Hawaii, NASA, ARC, Honolulu, HI 96822 USA.
EM hermalyn@hawaii.edu
NR 3
TC 0
Z9 0
U1 0
U2 0
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 1086-9379
EI 1945-5100
J9 METEORIT PLANET SCI
JI Meteorit. Planet. Sci.
PD SEP
PY 2014
VL 49
SU 1
SI SI
BP A163
EP A163
PG 1
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA AP2PA
UT WOS:000341914200160
ER
PT J
AU Jones, JH
Franz, HB
AF Jones, J. H.
Franz, H. B.
TI CORRELATIONS BETWEEN SURFICIAL SULFUR AND A CRUSTAL ASSIMILATION
SIGNATURE IN MARTIAN SHERGOTTITES
SO METEORITICS & PLANETARY SCIENCE
LA English
DT Meeting Abstract
CT 77th Annual Meeting of the Meteoritical-Society
CY SEP 08-13, 2014
CL Casablanca, MOROCCO
SP Meteorit Soc
C1 [Jones, J. H.] NASA JSC, KR, Houston, TX 77058 USA.
[Franz, H. B.] NASA GSFC, CRESST, Greenbelt, MD 20771 USA.
EM john.h.jones@nasa.gov
NR 1
TC 0
Z9 0
U1 0
U2 0
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 1086-9379
EI 1945-5100
J9 METEORIT PLANET SCI
JI Meteorit. Planet. Sci.
PD SEP
PY 2014
VL 49
SU 1
SI SI
BP A190
EP A190
PG 1
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA AP2PA
UT WOS:000341914200187
ER
PT J
AU Kebukawa, Y
Zolensky, ME
Fries, M
Kilcoyne, ALD
Rahman, Z
Cody, GD
AF Kebukawa, Y.
Zolensky, M. E.
Fries, M.
Kilcoyne, A. L. D.
Rahman, Z.
Cody, G. D.
TI DIVERSITY IN C-XANES SPECTRA OBTAINED FROM CARBONACEOUS SOLID INCLUSIONS
FROM MONAHANS HALITE.
SO METEORITICS & PLANETARY SCIENCE
LA English
DT Meeting Abstract
CT 77th Annual Meeting of the Meteoritical-Society
CY SEP 08-13, 2014
CL Casablanca, MOROCCO
SP Meteorit Soc
C1 [Kebukawa, Y.] Yokohama Natl Univ, Fac Engn, Yokohama, Kanagawa, Japan.
[Zolensky, M. E.; Fries, M.] NASA Johnson Space Ctr, Houston, TX USA.
[Kilcoyne, A. L. D.] Lawrence Berkeley Natl Lab, Adv Light Source, Berkeley, CA USA.
[Cody, G. D.] Carnegie Inst Sci, Geophys Lab, Washington, DC USA.
EM kebukawa@ynu.ac.jp
RI Kilcoyne, David/I-1465-2013
NR 3
TC 0
Z9 0
U1 0
U2 0
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 1086-9379
EI 1945-5100
J9 METEORIT PLANET SCI
JI Meteorit. Planet. Sci.
PD SEP
PY 2014
VL 49
SU 1
SI SI
BP A199
EP A199
PG 1
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA AP2PA
UT WOS:000341914200196
ER
PT J
AU Keller, LP
Berger, EL
AF Keller, L. P.
Berger, E. L.
TI SPACE WEATHERING OF OLIVINE IN LUNAR SOILS: A COMPARISON TO ITOKAWA
REGOLITH SAMPLES.
SO METEORITICS & PLANETARY SCIENCE
LA English
DT Meeting Abstract
CT 77th Annual Meeting of the Meteoritical-Society
CY SEP 08-13, 2014
CL Casablanca, MOROCCO
SP Meteorit Soc
C1 [Keller, L. P.] NASA JSC, Code KR, Houston, TX 77058 USA.
[Berger, E. L.] NASA JSC, Jacobs JETS Contract, GeoControl Syst Inc, Houston, TX 77058 USA.
EM Lindsay.P.Keller@nasa.gov
NR 3
TC 0
Z9 0
U1 2
U2 3
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 1086-9379
EI 1945-5100
J9 METEORIT PLANET SCI
JI Meteorit. Planet. Sci.
PD SEP
PY 2014
VL 49
SU 1
SI SI
BP A200
EP A200
PG 1
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA AP2PA
UT WOS:000341914200197
ER
PT J
AU Keller, LP
Needham, AW
Messenger, S
AF Keller, L. P.
Needham, A. W.
Messenger, S.
TI A FIB/TEM/NANOSIMS STUDY OF A WARK-LOVERING RIM ON AN ALLENDE CAI.
SO METEORITICS & PLANETARY SCIENCE
LA English
DT Meeting Abstract
CT 77th Annual Meeting of the Meteoritical-Society
CY SEP 08-13, 2014
CL Casablanca, MOROCCO
SP Meteorit Soc
C1 [Keller, L. P.; Messenger, S.] NASA JSC, Robert M Walker Lab Space Sci, Code KR, ARES, Houston, TX 77058 USA.
[Needham, A. W.] LPI, Houston, TX 77058 USA.
EM Lind-say.P.Keller@nasa.gov
NR 4
TC 0
Z9 0
U1 0
U2 2
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 1086-9379
EI 1945-5100
J9 METEORIT PLANET SCI
JI Meteorit. Planet. Sci.
PD SEP
PY 2014
VL 49
SU 1
SI SI
BP A201
EP A201
PG 1
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA AP2PA
UT WOS:000341914200198
ER
PT J
AU Liu, Y
Howarth, G
Young, ED
Pernet-Fisher, J
Kohl, I
Day, JMD
Chen, Y
Taylor, LA
AF Liu, Y.
Howarth, G.
Young, E. D.
Pernet-Fisher, J.
Kohl, I.
Day, J. M. D.
Chen, Y.
Taylor, L. A.
TI New olivine-phyric shergottites, Larkman Nunatuks (LAR) 12011, 12095,
12240
SO METEORITICS & PLANETARY SCIENCE
LA English
DT Meeting Abstract
CT 77th Annual Meeting of the Meteoritical-Society
CY SEP 08-13, 2014
CL Casablanca, MOROCCO
SP Meteorit Soc
C1 [Liu, Y.; Chen, Y.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Howarth, G.; Pernet-Fisher, J.; Taylor, L. A.] Univ Tennessee, Planetary Geosci Inst, Knoxville, TN 37996 USA.
[Young, E. D.; Kohl, I.] Univ Calif Los Angeles, Dept Earth Planet & Space Sci, Los Angeles, CA 90095 USA.
[Day, J. M. D.] Univ Calif San Diego, Scripps Inst Oceanog, La Jolla, CA 92093 USA.
EM yangliu@jpl.nasa.gov
NR 2
TC 0
Z9 0
U1 1
U2 1
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 1086-9379
EI 1945-5100
J9 METEORIT PLANET SCI
JI Meteorit. Planet. Sci.
PD SEP
PY 2014
VL 49
SU 1
SI SI
BP A240
EP A240
PG 1
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA AP2PA
UT WOS:000341914200237
ER
PT J
AU Ma, C
Tschauner, O
Beckett, JR
Liu, Y
Rossman, GR
Zuravlev, K
Prakapenka, V
Dera, P
Taylor, LA
AF Ma, C.
Tschauner, O.
Beckett, J. R.
Liu, Y.
Rossman, G. R.
Zuravlev, K.
Prakapenka, V.
Dera, P.
Taylor, L. A.
TI TISSINTITE, (Ca,Na,square)AlSi2O6: A SHOCK-INDUCED CLINOPYROXENE IN THE
TISSINT METEORITE.
SO METEORITICS & PLANETARY SCIENCE
LA English
DT Meeting Abstract
CT 77th Annual Meeting of the Meteoritical-Society
CY SEP 08-13, 2014
CL Casablanca, MOROCCO
SP Meteorit Soc
C1 [Ma, C.; Beckett, J. R.; Rossman, G. R.] CALTECH, Pasadena, CA 91125 USA.
[Tschauner, O.] Univ Nevada, Las Vegas, NV 89154 USA.
[Liu, Y.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Zuravlev, K.; Prakapenka, V.] Argonne Natl Lab, Argonne, IL 60439 USA.
[Dera, P.] Univ Hawaii Manoa, Honolulu, HI 96822 USA.
[Taylor, L. A.] Univ Tennessee, Knoxville, TN 37996 USA.
NR 4
TC 0
Z9 0
U1 2
U2 7
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 1086-9379
EI 1945-5100
J9 METEORIT PLANET SCI
JI Meteorit. Planet. Sci.
PD SEP
PY 2014
VL 49
SU 1
SI SI
BP A249
EP A249
PG 1
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA AP2PA
UT WOS:000341914200246
ER
PT J
AU Matsuno, J
Miyake, A
Tsuchiyama, A
Nakamura-Messenger, K
Messenger, S
AF Matsuno, J.
Miyake, A.
Tsuchiyama, A.
Nakamura-Messenger, K.
Messenger, S.
TI NANO-SCALE 3D OBSERVATION OF GEMS GRAINS
SO METEORITICS & PLANETARY SCIENCE
LA English
DT Meeting Abstract
CT 77th Annual Meeting of the Meteoritical-Society
CY SEP 08-13, 2014
CL Casablanca, MOROCCO
SP Meteorit Soc
ID ORIGINS
C1 [Matsuno, J.; Miyake, A.; Tsuchiyama, A.] Kyoto Univ, Dept Geol & Mineral, Kyoto 6068501, Japan.
[Nakamura-Messenger, K.; Messenger, S.] NASA Johnson Space Ctr, Houston, TX USA.
EM jmatsuno@kueps.kyoto-u.ac.jp
NR 5
TC 0
Z9 0
U1 0
U2 2
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 1086-9379
EI 1945-5100
J9 METEORIT PLANET SCI
JI Meteorit. Planet. Sci.
PD SEP
PY 2014
VL 49
SU 1
SI SI
BP A267
EP A267
PG 1
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA AP2PA
UT WOS:000341914200264
ER
PT J
AU McCubbin, FM
Tartese, R
Santos, AR
Domokos, G
Muttik, N
Szabo, T
Vazquez, J
Boyce, JW
Keller, LP
Jerolmack, DJ
Anand, M
Moser, DE
Delhaye, T
Shearer, CK
Agee, CB
AF McCubbin, F. M.
Tartese, R.
Santos, A. R.
Domokos, G.
Muttik, N.
Szabo, T.
Vazquez, J.
Boyce, J. W.
Keller, L. P.
Jerolmack, D. J.
Anand, M.
Moser, D. E.
Delhaye, T.
Shearer, C. K.
Agee, C. B.
TI ALTERATION OF SEDIMENTARY CLASTS IN MARTIAN METEORITE NORTHWEST AFRICA
7034
SO METEORITICS & PLANETARY SCIENCE
LA English
DT Meeting Abstract
CT 77th Annual Meeting of the Meteoritical-Society
CY SEP 08-13, 2014
CL Casablanca, MOROCCO
SP Meteorit Soc
C1 [McCubbin, F. M.; Santos, A. R.; Muttik, N.; Shearer, C. K.; Agee, C. B.] Univ New Mexico, Inst Meteorit, Albuquerque, NM 87131 USA.
[Tartese, R.; Anand, M.] Open Univ, Milton Keynes MK7 6AA, Bucks, England.
[Domokos, G.; Szabo, T.] Budapest Univ Technol & Econ, Dept Mech Mat & Struct, Budapest, Hungary.
[Vazquez, J.] US Geol Survey, Menlo Pk, CA 94025 USA.
[Vazquez, J.] Stanford Univ, Stanford USGS Ion Microprobe Lab, Stanford, CA 94305 USA.
[Boyce, J. W.] Univ Calif Los Angeles, Dept Earth & Space Sci, Los Angeles, CA 90095 USA.
[Keller, L. P.] NASA Johnson Space Ctr, Houston, TX 77058 USA.
[Jerolmack, D. J.] Univ Penn, Dept Earth & Environm Sci, Philadelphia, PA 19104 USA.
[Anand, M.] Nat Hist Museum, Dept Earth Sci, London SW7 5BD, England.
[Moser, D. E.] Univ Western Ontario, Dept Earth Sci, London, ON N6A 5B7, Canada.
[Delhaye, T.] Univ Rennes 1, Plateforme ONIS NanoSIMS, F-35042 Rennes, France.
EM fmccubbi@unm.edu
NR 1
TC 1
Z9 1
U1 0
U2 4
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 1086-9379
EI 1945-5100
J9 METEORIT PLANET SCI
JI Meteorit. Planet. Sci.
PD SEP
PY 2014
VL 49
SU 1
SI SI
BP A269
EP A269
PG 1
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA AP2PA
UT WOS:000341914200266
ER
PT J
AU Mikouchi, T
Aoyagi, Y
Sugiyama, K
Yokoyama, Y
Goodrich, CA
Zolensky, ME
AF Mikouchi, T.
Aoyagi, Y.
Sugiyama, K.
Yokoyama, Y.
Goodrich, C. A.
Zolensky, M. E.
TI EXPERIMENTAL CRYSTALLIZATION OF IRON MARTENSITE IN THE ALMAHATA SITTA
UREILITE.
SO METEORITICS & PLANETARY SCIENCE
LA English
DT Meeting Abstract
CT 77th Annual Meeting of the Meteoritical-Society
CY SEP 08-13, 2014
CL Casablanca, MOROCCO
SP Meteorit Soc
ID IMPACT
C1 [Mikouchi, T.; Aoyagi, Y.] Univ Tokyo, Dept Earth & Planet Sci, Tokyo 1130033, Japan.
[Sugiyama, K.; Yokoyama, Y.] Tohoku Univ, Inst Mat Res, Katahira, Miyagi 9808577, Japan.
[Goodrich, C. A.] Planet Sci Inst, Tucson, AZ 85719 USA.
[Zolensky, M. E.] NASA JSC, ARES, Houston, TX 77058 USA.
EM mikou-chi@eps.s.u-tokyo.ac.jp
RI Sugiyama, Kazumasa/B-3447-2010
NR 4
TC 0
Z9 0
U1 0
U2 0
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 1086-9379
EI 1945-5100
J9 METEORIT PLANET SCI
JI Meteorit. Planet. Sci.
PD SEP
PY 2014
VL 49
SU 1
SI SI
BP A282
EP A282
PG 1
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA AP2PA
UT WOS:000341914200279
ER
PT J
AU Mills, RD
Simon, JI
Wang, J
Hauri, EH
Alexander, CMO
AF Mills, R. D.
Simon, J. I.
Wang, J.
Hauri, E. H.
Alexander, C. M. O'D.
TI WATER CONTENT OF LUNAR ALKALI FELDSPAR.
SO METEORITICS & PLANETARY SCIENCE
LA English
DT Meeting Abstract
CT 77th Annual Meeting of the Meteoritical-Society
CY SEP 08-13, 2014
CL Casablanca, MOROCCO
SP Meteorit Soc
ID MOON
C1 [Mills, R. D.; Simon, J. I.] NASA, Ctr Isotope Cosmochem & Geochronol, ARES, JSC, Houston, TX 77058 USA.
[Wang, J.; Hauri, E. H.; Alexander, C. M. O'D.] Carnegie Inst Sci, DTM, Washington, DC 20015 USA.
EM rdmills25@gmail.com
NR 10
TC 0
Z9 0
U1 0
U2 2
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 1086-9379
EI 1945-5100
J9 METEORIT PLANET SCI
JI Meteorit. Planet. Sci.
PD SEP
PY 2014
VL 49
SU 1
SI SI
BP A284
EP A284
PG 1
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA AP2PA
UT WOS:000341914200281
ER
PT J
AU Mittlefehldt, DW
AF Mittlefehldt, D. W.
TI HOWARDITES AND MESOSIDERITES: CONTRASTING POLYMICT BRECCIAS FROM TWO
SIMILAR DIFFERENTIATED ASTEROIDS.
SO METEORITICS & PLANETARY SCIENCE
LA English
DT Meeting Abstract
CT 77th Annual Meeting of the Meteoritical-Society
CY SEP 08-13, 2014
CL Casablanca, MOROCCO
SP Meteorit Soc
ID CONSTRAINTS; LITHOLOGIES; HISTORY; CLASTS
C1 [Mittlefehldt, D. W.] NASA, Lyndon B Johnson Space Ctr, Astromat Res Off, Houston, TX 77058 USA.
EM david.w.mittlefehldt@nasa.gov
NR 12
TC 0
Z9 0
U1 0
U2 0
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 1086-9379
EI 1945-5100
J9 METEORIT PLANET SCI
JI Meteorit. Planet. Sci.
PD SEP
PY 2014
VL 49
SU 1
SI SI
BP A285
EP A285
PG 1
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA AP2PA
UT WOS:000341914200282
ER
PT J
AU Nagao, K
Haba, MK
Zolensky, M
Jenniskens, P
Shaddad, MH
AF Nagao, K.
Haba, M. K.
Zolensky, M.
Jenniskens, P.
Shaddad, M. H.
TI NOBLE GASES IN TWO FRAGMENTS OF DIFFERENT LITHOLOGIES FROM THE ALMAHATA
SITTA METEORITE.
SO METEORITICS & PLANETARY SCIENCE
LA English
DT Meeting Abstract
CT 77th Annual Meeting of the Meteoritical-Society
CY SEP 08-13, 2014
CL Casablanca, MOROCCO
SP Meteorit Soc
ID ASTEROID 2008 TC3; UREILITE; RECOVERY
C1 [Nagao, K.] Univ Tokyo, Geochem Res Ctr, Tokyo 1130033, Japan.
[Haba, M. K.] NIPR, Tokyo 1908518, Japan.
[Zolensky, M.] NASA, Lyndon B Johnson Space Ctr, ARES, Houston, TX 77058 USA.
[Jenniskens, P.] SETI Inst, Mountain View, CA 94043 USA.
[Shaddad, M. H.] Univ Khartoum, Phys & Astron Dept, Khartoum 11115, Sudan.
EM nagao@eqchem.s.u-tokyo.ac.jp
NR 12
TC 0
Z9 0
U1 0
U2 3
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 1086-9379
EI 1945-5100
J9 METEORIT PLANET SCI
JI Meteorit. Planet. Sci.
PD SEP
PY 2014
VL 49
SU 1
SI SI
BP A294
EP A294
PG 1
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA AP2PA
UT WOS:000341914200291
ER
PT J
AU Nguyen, AN
Berger, EL
Nakamura-Messenger, K
Messenger, S
AF Nguyen, A. N.
Berger, E. L.
Nakamura-Messenger, K.
Messenger, S.
TI COORDINATED MINERALOGICAL AND ISOTOPIC ANALYSIS OF A COSMIC SYMPLECTITE
IDENTIFIED IN A STARDUST TERMINAL PARTICLE.
SO METEORITICS & PLANETARY SCIENCE
LA English
DT Meeting Abstract
CT 77th Annual Meeting of the Meteoritical-Society
CY SEP 08-13, 2014
CL Casablanca, MOROCCO
SP Meteorit Soc
ID TRACKS
C1 [Nguyen, A. N.; Berger, E. L.] NASA, Lyndon B Johnson Space Ctr, JETS, Houston, TX 77058 USA.
[Nguyen, A. N.; Berger, E. L.; Nakamura-Messenger, K.; Messenger, S.] NASA, Lyndon B Johnson Space Ctr, Robert M Walker Lab Space Sci, ARES, Houston, TX 77058 USA.
EM lan-anh.n.nguyen@nasa.gov
NR 8
TC 0
Z9 0
U1 0
U2 0
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 1086-9379
EI 1945-5100
J9 METEORIT PLANET SCI
JI Meteorit. Planet. Sci.
PD SEP
PY 2014
VL 49
SU 1
SI SI
BP A298
EP A298
PG 1
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA AP2PA
UT WOS:000341914200295
ER
PT J
AU Nuth, JA
Johnson, NM
Carayon, A
AF Nuth, Joseph A.
Johnson, Natasha M.
Carayon, Alicia
TI MEASURING VOLATILE/SOLID CARBON BRANCHING RATIOS FOR
FISCHER-TROPSCH-TYPE REACTIONS.
SO METEORITICS & PLANETARY SCIENCE
LA English
DT Meeting Abstract
CT 77th Annual Meeting of the Meteoritical-Society
CY SEP 08-13, 2014
CL Casablanca, MOROCCO
SP Meteorit Soc
ID SOLAR NEBULA; CHEMISTRY; CATALYSIS
C1 [Nuth, Joseph A.] NASA, Goddard Space Flight Ctr, Solar Syst Explorat Div, Washington, DC USA.
[Johnson, Natasha M.; Carayon, Alicia] NASA, Goddard Space Flight Ctr, Astrochem Lab, Washington, DC USA.
[Carayon, Alicia] Int Space Univ, Illkirch Graffenstaden, France.
EM joseph.a.nuth@nasa.gov
RI Johnson, Natasha/E-3093-2012
NR 8
TC 0
Z9 0
U1 0
U2 0
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 1086-9379
EI 1945-5100
J9 METEORIT PLANET SCI
JI Meteorit. Planet. Sci.
PD SEP
PY 2014
VL 49
SU 1
SI SI
BP A301
EP A301
PG 1
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA AP2PA
UT WOS:000341914200298
ER
PT J
AU Park, J
Nyquist, LE
Herzog, GF
Turrin, BD
Lindsay, FN
Delaney, JS
Swisher, CC
Shih, CY
Shirai, N
Yamaguchi, A
AF Park, J.
Nyquist, L. E.
Herzog, G. F.
Turrin, B. D.
Lindsay, F. N.
Delaney, J. S.
Swisher, C. C., III
Shih, C. -Y.
Shirai, N.
Yamaguchi, A.
TI Ar-40/Ar-39 AGES OF ANORTHOSITIC LUNAR ROCK 64435
SO METEORITICS & PLANETARY SCIENCE
LA English
DT Meeting Abstract
CT 77th Annual Meeting of the Meteoritical-Society
CY SEP 08-13, 2014
CL Casablanca, MOROCCO
SP Meteorit Soc
C1 [Park, J.; Herzog, G. F.; Turrin, B. D.; Lindsay, F. N.; Delaney, J. S.; Swisher, C. C., III] Rutgers U, Piscataway, NJ 08854 USA.
[Park, J.] LPI, Houston, TX 77058 USA.
[Park, J.] Kingsborough Comm Coll, Brooklyn, NY 11235 USA.
[Nyquist, L. E.] KR NASA Johnson Space Ctr, Houston, TX 77058 USA.
[Shih, C. -Y.] Jacobs, Houston, TX 77258 USA.
[Shirai, N.] Tokyo Metropolitan Univ, Hachioji, Tokyo 1920372, Japan.
[Yamaguchi, A.] NIPR Tokyo, AMRC, Tokyo 1908518, Japan.
NR 9
TC 0
Z9 0
U1 0
U2 3
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 1086-9379
EI 1945-5100
J9 METEORIT PLANET SCI
JI Meteorit. Planet. Sci.
PD SEP
PY 2014
VL 49
SU 1
SI SI
BP A316
EP A316
PG 1
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA AP2PA
UT WOS:000341914200313
ER
PT J
AU Povenmire, H
Lehrman, N
Zolensky, M
AF Povenmire, H.
Lehrman, N.
Zolensky, M.
TI THE DUMBBELL, LAYERED INTERNAL SCHLIEREN TEKTITE FROM CHINA
SO METEORITICS & PLANETARY SCIENCE
LA English
DT Meeting Abstract
CT 77th Annual Meeting of the Meteoritical-Society
CY SEP 08-13, 2014
CL Casablanca, MOROCCO
SP Meteorit Soc
C1 [Povenmire, H.] FL Inst Technol, Indialantic, FL 32903 USA.
[Zolensky, M.] NASA JSC, ARES, Houston, TX 77058 USA.
EM katiehall@yahoo.com
NR 1
TC 0
Z9 0
U1 0
U2 0
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 1086-9379
EI 1945-5100
J9 METEORIT PLANET SCI
JI Meteorit. Planet. Sci.
PD SEP
PY 2014
VL 49
SU 1
SI SI
BP A327
EP A327
PG 1
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA AP2PA
UT WOS:000341914200324
ER
PT J
AU Rampino, MR
AF Rampino, Michael R.
TI DISC DARK MATTER IN THE GALAXY AND CYCLES OF EXTRATERRESTRIAL IMPACTS,
MASS EXTINCTIONS AND GEOTECTONIC EVENTS
SO METEORITICS & PLANETARY SCIENCE
LA English
DT Meeting Abstract
CT 77th Annual Meeting of the Meteoritical-Society
CY SEP 08-13, 2014
CL Casablanca, MOROCCO
SP Meteorit Soc
C1 [Rampino, Michael R.] NYU, Dept Biol & Environm Studies, New York, NY 10003 USA.
[Rampino, Michael R.] NASA, Goddard Inst Space Studies, New York, NY 10027 USA.
EM mrr1@nyu.edu
NR 0
TC 0
Z9 0
U1 2
U2 5
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 1086-9379
EI 1945-5100
J9 METEORIT PLANET SCI
JI Meteorit. Planet. Sci.
PD SEP
PY 2014
VL 49
SU 1
SI SI
BP A334
EP A334
PG 1
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA AP2PA
UT WOS:000341914200331
ER
PT J
AU Sandford, SA
Materese, CK
Nuevo, M
AF Sandford, S. A.
Materese, C. K.
Nuevo, M.
TI FORMATION OF HETEROCYCLES FROM THE UV IRRADIATION OF POLYCYCLIC AROMATIC
HYDROCARBONS IN ICES.
SO METEORITICS & PLANETARY SCIENCE
LA English
DT Meeting Abstract
CT 77th Annual Meeting of the Meteoritical-Society
CY SEP 08-13, 2014
CL Casablanca, MOROCCO
SP Meteorit Soc
ID ULTRAVIOLET PHOTOIRRADIATION; NUCLEOBASES; PYRIMIDINE; PHOTOLYSIS;
ANALOGS
C1 [Sandford, S. A.; Materese, C. K.; Nuevo, M.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Materese, C. K.] Oak Ridge Associated Univ, Oak Ridge, TN USA.
[Nuevo, M.] Bay Area Environm Res Inst, Petaluma, CA USA.
EM Scott.A.Sandford@nasa.gov
NR 7
TC 0
Z9 0
U1 1
U2 3
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 1086-9379
EI 1945-5100
J9 METEORIT PLANET SCI
JI Meteorit. Planet. Sci.
PD SEP
PY 2014
VL 49
SU 1
SI SI
BP A353
EP A353
PG 1
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA AP2PA
UT WOS:000341914200350
ER
PT J
AU Simon, JI
Peters, TJ
Tappa, MJ
Agee, CB
AF Simon, J. I.
Peters, T. J.
Tappa, M. J.
Agee, C. B.
TI NORTHWEST AFRICA 8159: AN similar to 2.3 BILLION YEAR OLD MARTIAN
OLIVINE-BEARING AUGITE BASALT
SO METEORITICS & PLANETARY SCIENCE
LA English
DT Meeting Abstract
CT 77th Annual Meeting of the Meteoritical-Society
CY SEP 08-13, 2014
CL Casablanca, MOROCCO
SP Meteorit Soc
C1 [Simon, J. I.; Peters, T. J.; Tappa, M. J.] NASA, Lyndon B Johnson Space Ctr, Ctr Isotope Cosmochem & Geochronol Astromat Res &, Houston, TX 77058 USA.
[Peters, T. J.] Lunar & Planetary Inst, Houston, TX 77058 USA.
[Tappa, M. J.] JETS Jacobs Technol, Houston, TX 77258 USA.
[Agee, C. B.] Univ New Mexico, Inst Meteorit, Albuquerque, NM 87131 USA.
EM Justin.I.Simon@NASA.gov
NR 4
TC 0
Z9 0
U1 1
U2 1
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 1086-9379
EI 1945-5100
J9 METEORIT PLANET SCI
JI Meteorit. Planet. Sci.
PD SEP
PY 2014
VL 49
SU 1
SI SI
BP A363
EP A363
PG 1
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA AP2PA
UT WOS:000341914200360
ER
PT J
AU Smith, RL
Blake, GA
Boogert, ACA
Pontoppidan, KM
Lockwood, AC
AF Smith, R. L.
Blake, G. A.
Boogert, A. C. A.
Pontoppidan, K. M.
Lockwood, A. C.
TI INVESTIGATING PROTOSTELLAR CARBON RESERVOIRS WITH HIGH-RESOLUTION
SPECTROSCOPY TOWARD MASSIVE YOUNG STELLAR OBJECTS
SO METEORITICS & PLANETARY SCIENCE
LA English
DT Meeting Abstract
CT 77th Annual Meeting of the Meteoritical-Society
CY SEP 08-13, 2014
CL Casablanca, MOROCCO
SP Meteorit Soc
ID CO2
C1 [Smith, R. L.] NC Museum Nat Sci, Raleigh, NC USA.
[Smith, R. L.] Appalachian State Univ, Boone, NC 28608 USA.
[Blake, G. A.; Lockwood, A. C.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA.
[Boogert, A. C. A.] NASA Ames, SOFIA USRA, Ames, IA USA.
[Pontoppidan, K. M.] Space Telescope Sci Inst, Baltimore, MD USA.
EM rachel.smith@naturalsciences.org
NR 9
TC 0
Z9 0
U1 1
U2 3
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 1086-9379
EI 1945-5100
J9 METEORIT PLANET SCI
JI Meteorit. Planet. Sci.
PD SEP
PY 2014
VL 49
SU 1
SI SI
BP A370
EP A370
PG 1
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA AP2PA
UT WOS:000341914200367
ER
PT J
AU Steele, A
McCubbin, FM
Benning, LG
Siljestrom, S
Cody, GD
Goreva, Y
Hauri, EH
Wang, J
Kilcoyne, ALD
Grady, M
Verchovsky, A
Sabbah, H
Smith, C
Freissinet, C
Glavin, DP
Burton, AS
Fries, MD
Blanco, JDR
Glamoclija, M
Rogers, KL
Mikhail, S
Zare, RN
Wu, Q
Ismail, A
Dworkin, JP
Bhartia, R
AF Steele, A.
McCubbin, F. M.
Benning, L. G.
Siljestroem, S.
Cody, G. D.
Goreva, Y.
Hauri, E. H.
Wang, J.
Kilcoyne, A. L. D.
Grady, M.
Verchovsky, A.
Sabbah, H.
Smith, C.
Freissinet, C.
Glavin, D. P.
Burton, A. S.
Fries, M. D.
Blanco, Rodriguez J. D.
Glamoclija, M.
Rogers, K. L.
Mikhail, S.
Zare, R. N.
Wu, Q.
Ismail, A.
Dworkin, J. P.
Bhartia, R.
TI Hydrothermal Organic Synthesis on Mars: Evidence from the Tissint
Meteorite
SO METEORITICS & PLANETARY SCIENCE
LA English
DT Meeting Abstract
CT 77th Annual Meeting of the Meteoritical-Society
CY SEP 08-13, 2014
CL Casablanca, MOROCCO
SP Meteorit Soc
C1 [Steele, A.; Siljestroem, S.; Cody, G. D.; Glamoclija, M.; Rogers, K. L.] Carnegie Inst Sci, Geophys Lab, Washington, DC 20015 USA.
[McCubbin, F. M.] Univ New Mexico, Dept Earth & Planetary Sci, Inst Meteorit, Albuquerque, NM 87131 USA.
[Benning, L. G.; Blanco, Rodriguez J. D.] Univ Leeds, Sch Earth & Environm, Leeds LS2 9JT, W Yorkshire, England.
[Siljestroem, S.] SP Tech Res Inst Sweden, Dept Chem Mat & Surfaces, Boras, Sweden.
[Siljestroem, S.; Goreva, Y.] Smithsonian Inst, Dept Mineral Sci, Washington, DC 20560 USA.
[Hauri, E. H.; Wang, J.] Carnegie Inst Sci, Dept Terr Magnetism, Washington, DC 20015 USA.
[Kilcoyne, A. L. D.] Adv Light Source, Berkeley, CA USA.
[Grady, M.; Verchovsky, A.] Stanford Univ, Ctr Earth Planetary Space & Astron Res, Stanford, CA 94305 USA.
[Sabbah, H.; Zare, R. N.; Wu, Q.; Ismail, A.] Stanford Univ, Dept Chem, Stanford, CA 94305 USA.
[Sabbah, H.] Univ Toulouse, Toulouse, France.
[Sabbah, H.] CNRS, Toulouse, France.
[Smith, C.] Nat Hist Museum, Dept Mineral, London, England.
[Freissinet, C.; Glavin, D. P.; Dworkin, J. P.] NASA, Goddard Space Flight Ctr, Houston, TX USA.
[Burton, A. S.; Fries, M. D.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA.
[Blanco, Rodriguez J. D.] Univ Copenhagen, Dept Chem, Nanosci Ctr, DK-1168 Copenhagen, Denmark.
[Glamoclija, M.] Rutgers State Univ, Dept Earth & Planetary Sci, Piscataway, NJ 08855 USA.
[Rogers, K. L.] Rensselaer Polytech Inst, Troy, NY 12181 USA.
[Mikhail, S.] Univ Edinburgh, Sch Geosci, Edinburgh EH8 9YL, Midlothian, Scotland.
[Ismail, A.] King Abdulaziz Univ, Dept Chem, Rabigh, Saudi Arabia.
[Bhartia, R.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
RI Ismail, Ali/I-7595-2012; Glavin, Daniel/D-6194-2012; Kilcoyne,
David/I-1465-2013; Dworkin, Jason/C-9417-2012
OI Ismail, Ali/0000-0001-9556-5140; Glavin, Daniel/0000-0001-7779-7765;
Dworkin, Jason/0000-0002-3961-8997
NR 0
TC 1
Z9 1
U1 1
U2 16
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 1086-9379
EI 1945-5100
J9 METEORIT PLANET SCI
JI Meteorit. Planet. Sci.
PD SEP
PY 2014
VL 49
SU 1
SI SI
BP A376
EP A376
PG 1
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA AP2PA
UT WOS:000341914200373
ER
PT J
AU Trivedi, M
Smith, HD
Sears, DWG
AF Trivedi, M.
Smith, H. D.
Sears, D. W. G.
TI DETECTING AND DISTINGUISHING METAMORPHIC GRADIENTS OF UNEQUILIBRATED
(TYPE 3) ORDINARY CHONDRITES USING INFRARED REFLECTANCE SPECTRA
SO METEORITICS & PLANETARY SCIENCE
LA English
DT Meeting Abstract
CT 77th Annual Meeting of the Meteoritical-Society
CY SEP 08-13, 2014
CL Casablanca, MOROCCO
SP Meteorit Soc
C1 [Trivedi, M.; Smith, H. D.; Sears, D. W. G.] NASA, Ames Res Ctr, Space Sci & Astrobiol Div, Moffett Field, CA 94035 USA.
EM Mi-hir.Trivedi17@bcp.org; Heather.d.smith@nasa.gov; derek.sears@nasa.gov
NR 4
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
EI 1945-5100
J9 METEORIT PLANET SCI
JI Meteorit. Planet. Sci.
PD SEP
PY 2014
VL 49
SU 1
SI SI
BP A403
EP A403
PG 1
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA AP2PA
UT WOS:000341914200400
ER
PT J
AU Tsuchiyama, A
Miyake, A
Zolensky, ME
Uesugi, K
Nakano, T
Takeuchi, A
Suzuki, Y
Yoshida, K
AF Tsuchiyama, A.
Miyake, A.
Zolensky, M. E.
Uesugi, K.
Nakano, T.
Takeuchi, A.
Suzuki, Y.
Yoshida, K.
TI SEARCH FOR FLUID INCLUSIONS IN A CARBONACEOUS CHONDRITE USING A NEW
X-RAY MICRO-TOMOGRAPHY TECHNIQUE COMBAINED WITH FIB SAMPLING.
SO METEORITICS & PLANETARY SCIENCE
LA English
DT Meeting Abstract
CT 77th Annual Meeting of the Meteoritical-Society
CY SEP 08-13, 2014
CL Casablanca, MOROCCO
SP Meteorit Soc
C1 [Tsuchiyama, A.; Miyake, A.; Yoshida, K.] Kyoto Univ, Grad Sch Sci, Kyoto 6068501, Japan.
[Zolensky, M. E.] NASA, JSC, Houston, TX USA.
[Uesugi, K.; Takeuchi, A.; Suzuki, Y.] SPring 8, JASRI, Koto, Hyogo, Japan.
[Nakano, T.] GSJ, AIST, Tsukuba, Ibaraki, Japan.
NR 4
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
EI 1945-5100
J9 METEORIT PLANET SCI
JI Meteorit. Planet. Sci.
PD SEP
PY 2014
VL 49
SU 1
SI SI
BP A404
EP A404
PG 1
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA AP2PA
UT WOS:000341914200401
ER
PT J
AU Uesugi, M
Tsuchiyama, A
Uesugi, K
Takeuchi, A
Suzuki, Y
Park, J
Nagao, K
Nishiizumi, K
Nakashima, D
Kita, N
Langenhorst, F
Keller, L
Karouji, Y
Nakato, A
Yada, T
Kumagai, K
Okada, T
Abe, M
AF Uesugi, M.
Tsuchiyama, A.
Uesugi, K.
Takeuchi, A.
Suzuki, Y.
Park, J.
Nagao, K.
Nishiizumi, K.
Nakashima, D.
Kita, N.
Langenhorst, F.
Keller, L.
Karouji, Y.
Nakato, A.
Yada, T.
Kumagai, K.
Okada, T.
Abe, M.
TI CURRENT STATUS OF THE CONSORTIUM STURDY OF THE LARGEST ITOKAWA PARTICLE
RA-QD02-0136-01
SO METEORITICS & PLANETARY SCIENCE
LA English
DT Meeting Abstract
CT 77th Annual Meeting of the Meteoritical-Society
CY SEP 08-13, 2014
CL Casablanca, MOROCCO
SP Meteorit Soc
C1 [Uesugi, M.; Karouji, Y.; Nakato, A.; Yada, T.; Kumagai, K.; Okada, T.; Abe, M.] Japan Aerosp Explorat Agcy JAXA, Inst Space & Astronaut Sci, Tokyo, Japan.
[Tsuchiyama, A.; Okada, T.; Abe, M.] Kyoto Univ, Kyoto 6068501, Japan.
[Uesugi, K.; Takeuchi, A.; Suzuki, Y.] Japan Synchrotron Radiat Inst JASRI, Tokyo, Japan.
[Park, J.] Rutgers State Univ, Piscataway, NJ 08855 USA.
[Nagao, K.] Univ Tokyo, Tokyo 1138654, Japan.
[Nishiizumi, K.] Univ Calif, Oakland, CA USA.
[Nakashima, D.] Tohoku Univ, Sendai, Miyagi 980, Japan.
[Kita, N.] Univ Wisconsin Madison, Madison, WI USA.
[Langenhorst, F.] Univ Jena, D-07745 Jena, Germany.
[Keller, L.] NASA, JSC, Houston, TX USA.
NR 8
TC 0
Z9 0
U1 1
U2 2
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 1086-9379
EI 1945-5100
J9 METEORIT PLANET SCI
JI Meteorit. Planet. Sci.
PD SEP
PY 2014
VL 49
SU 1
SI SI
BP A409
EP A409
PG 1
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA AP2PA
UT WOS:000341914200406
ER
PT J
AU Weisberg, MK
Zolensky, ME
Kimura, M
Ebel, DS
AF Weisberg, M. K.
Zolensky, M. E.
Kimura, M.
Ebel, D. S.
TI THE HIGHLY PRIMITIVE ALH 81189 EH3 CHONDRITE
SO METEORITICS & PLANETARY SCIENCE
LA English
DT Meeting Abstract
CT 77th Annual Meeting of the Meteoritical-Society
CY SEP 08-13, 2014
CL Casablanca, MOROCCO
SP Meteorit Soc
ID ENSTATITE CHONDRITES; EARTH
C1 [Weisberg, M. K.] Kingsborough Coll CUNY, Dept Phys Sci, Brooklyn, NY 11235 USA.
[Weisberg, M. K.; Ebel, D. S.] CUNY, Grad Ctr, New York, NY 10016 USA.
[Weisberg, M. K.; Ebel, D. S.] Amer Museum Nat Hist, Dept Earth & Planet Sci, New York, NY 10024 USA.
[Zolensky, M. E.] NASA, Lyndon B Johnson Space Ctr, ARES, Houston, TX 77058 USA.
[Kimura, M.] Ibaraki Univ, Fac Sci, Mito, Ibaraki 3108512, Japan.
[Kimura, M.] Natl Inst Polar Res, Tokyo 1908518, Japan.
NR 14
TC 0
Z9 0
U1 0
U2 2
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 1086-9379
EI 1945-5100
J9 METEORIT PLANET SCI
JI Meteorit. Planet. Sci.
PD SEP
PY 2014
VL 49
SU 1
SI SI
BP A429
EP A429
PG 1
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA AP2PA
UT WOS:000341914200426
ER
PT J
AU Wozniakiewicz, PJ
Bradley, JP
Price, MC
Zolensky, ME
Ishii, HA
Brownlee, DE
Russell, SS
AF Wozniakiewicz, P. J.
Bradley, J. P.
Price, M. C.
Zolensky, M. E.
Ishii, H. A.
Brownlee, D. E.
Russell, S. S.
TI CONTEMPORARY COSMIC DUST ARRIVING AT THE EARTH'S SURFACE: INITIAL
RESULTS FROM THE KWAJALEIN MICROMETEORITE COLLECTION.
SO METEORITICS & PLANETARY SCIENCE
LA English
DT Meeting Abstract
CT 77th Annual Meeting of the Meteoritical-Society
CY SEP 08-13, 2014
CL Casablanca, MOROCCO
SP Meteorit Soc
ID ACCRETION RATE
C1 [Wozniakiewicz, P. J.; Russell, S. S.] Nat Hist Museum, Dept Earth Sci, London SW7 5BD, England.
[Wozniakiewicz, P. J.; Price, M. C.] Univ Kent, Sch Phys Sci, Canterbury CT2 7NH, Kent, England.
[Bradley, J. P.; Ishii, H. A.] Univ Hawaii, Hawaii Inst Geophys & Planetol, Honolulu, HI 96822 USA.
[Zolensky, M. E.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA.
[Brownlee, D. E.] Univ Washington, Dept Astron, Seattle, WA 98195 USA.
EM p.wozniakiewicz@nhm.ac.uk
NR 6
TC 0
Z9 0
U1 1
U2 3
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 1086-9379
EI 1945-5100
J9 METEORIT PLANET SCI
JI Meteorit. Planet. Sci.
PD SEP
PY 2014
VL 49
SU 1
SI SI
BP A438
EP A438
PG 1
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA AP2PA
UT WOS:000341914200435
ER
PT J
AU Yabuta, H
Uesugi, M
Naraoka, H
Ito, M
Kilcoyne, D
Sandford, SA
Kitajima, F
Mita, H
Takano, Y
Yada, T
Karouji, Y
Ishibashi, Y
Okada, T
Abe, M
AF Yabuta, H.
Uesugi, M.
Naraoka, H.
Ito, M.
Kilcoyne, D.
Sandford, S. A.
Kitajima, F.
Mita, H.
Takano, Y.
Yada, T.
Karouji, Y.
Ishibashi, Y.
Okada, T.
Abe, M.
TI FUNCTIONAL GROUP COMPOSITIONS OF CARBONACEOUS MATERIALS OF
HAYABUSA-RETURNED SAMPLES.
SO METEORITICS & PLANETARY SCIENCE
LA English
DT Meeting Abstract
CT 77th Annual Meeting of the Meteoritical-Society
CY SEP 08-13, 2014
CL Casablanca, MOROCCO
SP Meteorit Soc
C1 [Yabuta, H.] Osaka Univ, Suita, Osaka 565, Japan.
[Uesugi, M.; Yada, T.; Karouji, Y.; Ishibashi, Y.; Okada, T.; Abe, M.] JAXA ISAS, Sagamihara, Kanagawa, Japan.
[Naraoka, H.; Kitajima, F.] Kyushu Univ, Fukuoka 812, Japan.
[Ito, M.; Takano, Y.] JAMSTEC, Yokosuka, Kanagawa, Japan.
[Kilcoyne, D.] LBNL, Adv Light Source, Berkeley, CA USA.
[Sandford, S. A.] NASA, Ames, IA USA.
[Mita, H.] Fukuoka Inst Tech Japan, Fukuoka, Japan.
EM hyabuta@ess.sci.osaka-u.ac.jp
RI Kilcoyne, David/I-1465-2013
NR 9
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
EI 1945-5100
J9 METEORIT PLANET SCI
JI Meteorit. Planet. Sci.
PD SEP
PY 2014
VL 49
SU 1
SI SI
BP A443
EP A443
PG 1
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA AP2PA
UT WOS:000341914200440
ER
PT J
AU Zeigler, RA
Almeida, NV
Sykes, D
Smith, CL
AF Zeigler, R. A.
Almeida, N. V.
Sykes, D.
Smith, C. L.
TI X-RAY MICRO-COMPUTED TOMOGRAPHY OF APOLLO SAMPLES AS A CURATION
TECHNIQUE ENABLING BETTER RESEARCH
SO METEORITICS & PLANETARY SCIENCE
LA English
DT Meeting Abstract
CT 77th Annual Meeting of the Meteoritical-Society
CY SEP 08-13, 2014
CL Casablanca, MOROCCO
SP Meteorit Soc
C1 [Zeigler, R. A.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA.
[Almeida, N. V.; Smith, C. L.] Nat Hist Museum, Dept Earth Sci, London, England.
[Sykes, D.] Nat Hist Museum, Imaging & Anal Ctr, London, England.
EM ryan.a.zeigler@nasa.gov
NR 4
TC 0
Z9 0
U1 0
U2 0
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 1086-9379
EI 1945-5100
J9 METEORIT PLANET SCI
JI Meteorit. Planet. Sci.
PD SEP
PY 2014
VL 49
SU 1
SI SI
BP A450
EP A450
PG 1
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA AP2PA
UT WOS:000341914200447
ER
PT J
AU Zolensky, M
Frank, D
AF Zolensky, M.
Frank, D.
TI SURVIVING HIGH-TEMPERATURE COMPONENTS IN CI CHONDRITES.
SO METEORITICS & PLANETARY SCIENCE
LA English
DT Meeting Abstract
CT 77th Annual Meeting of the Meteoritical-Society
CY SEP 08-13, 2014
CL Casablanca, MOROCCO
SP Meteorit Soc
C1 [Zolensky, M.] NASA, ARES, JSC, Houston, TX 77058 USA.
[Frank, D.] ESCG, Houston, TX 77058 USA.
EM michael.e.zolensky@nasa.gov
NR 3
TC 0
Z9 0
U1 0
U2 0
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 1086-9379
EI 1945-5100
J9 METEORIT PLANET SCI
JI Meteorit. Planet. Sci.
PD SEP
PY 2014
VL 49
SU 1
SI SI
BP A453
EP A453
PG 1
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA AP2PA
UT WOS:000341914200450
ER
PT J
AU Morscher, GN
Smith, C
Maillet, E
Baker, C
Monsour, R
AF Morscher, Gregory N.
Smith, Craig
Maillet, Emmanuel
Baker, Chris
Monsour, Rabih
TI Electrical resistance monitoring of damage and crack growth in advanced
SiC-based ceramic composites
SO AMERICAN CERAMIC SOCIETY BULLETIN
LA English
DT Article
ID MATRIX COMPOSITES
C1 [Morscher, Gregory N.; Maillet, Emmanuel; Monsour, Rabih] Univ Akron, Akron, OH 44325 USA.
[Smith, Craig] NASA, Glenn Res Ctr, Cleveland, OH USA.
[Baker, Chris] Bridgestone Amer Tire Operat, Akron, OH USA.
RP Morscher, GN (reprint author), Univ Akron, Akron, OH 44325 USA.
EM gm33@uakron.edu
OI Maillet, Emmanuel/0000-0001-5143-4982
FU ONR [N00014-11-1-0765]; Navy STTR [N68335-13-C-0349]; NASA Glenn
Research Center
FX ONR Contract No. N00014-11-1-0765 (William Nickerson PI), Navy STTR
Contract No. N68335-13-C-0349, and NASA Glenn Research Center funded
this work.
NR 10
TC 1
Z9 1
U1 0
U2 10
PU AMER CERAMIC SOC
PI WESTERVILLE
PA 600 N CLEVELAND AVE, WESTERVILLE, OH 43082 USA
SN 0002-7812
EI 1945-2705
J9 AM CERAM SOC BULL
JI Am. Ceram. Soc. Bull.
PD SEP
PY 2014
VL 93
IS 7
BP 28
EP 31
PG 4
WC Materials Science, Ceramics
SC Materials Science
GA AO8OV
UT WOS:000341615000019
ER
PT J
AU Jain, M
Jiang, AX
Kido, T
Takadama, K
Mercer, EG
Rungta, N
Waser, M
Wagner, A
Burke, J
Sofge, D
Lawless, W
Sridharan, M
Hawes, N
Hwang, T
AF Jain, Manish
Jiang, Albert Xin
Kido, Takashi
Takadama, Keiki
Mercer, Eric G.
Rungta, Neha
Waser, Mark
Wagner, Alan
Burke, Jennifer
Sofge, Don
Lawless, William
Sridharan, Mohan
Hawes, Nick
Hwang, Tim
TI Reports of the 2014 AAAI Spring Symposium Series
SO AI MAGAZINE
LA English
DT Article
AB The Association for the Advancement of Artificial Intelligence was pleased to present the AAAI 2014 Spring Symposium Series, held Monday through Wednesday, March 24-26, 2014. The titles of the eight symposia were Applied Computational Game Theory, Big Data Becomes Personal:, Knowledge into Meaning, Formal Verification and Modeling in Human-Machine Systems, Implementing Selves with Safe Motivational Systems and Self-Improvement, The Intersection of Robust Intelligence and Trust in Autonomous Systems, Knowledge Representation and Reasoning in Robotics, Qualitative Representations for Robots, and Social Hacking and Cognitive Security on the Internet and New Media). This report contains summaries of the symposia, written, in most cases, by the cochairs of the symposium.
C1 [Jain, Manish] Virginia Polytech Inst & State Univ, Dept Comp Sci, Blacksburg, VA 24061 USA.
[Jiang, Albert Xin] Univ So Calif, Dept Comp Sci, Los Angeles, CA 90089 USA.
[Kido, Takashi] Rikengenesis, Yokohama, Kanagawa, Japan.
[Takadama, Keiki] Univ Electrocommun, Chofu, Tokyo 182, Japan.
[Mercer, Eric G.] Brigham Young Univ, Dept Comp Sci, Provo, UT 84602 USA.
[Rungta, Neha] NASA, Ames Res Ctr, Moffett Field, CA USA.
[Waser, Mark] Digital Wisdom Inst, New York, NY USA.
[Wagner, Alan] Georgia Inst Technol, Georgia Tech Res Inst, Atlanta, GA 30332 USA.
[Burke, Jennifer] Boeing Res & Technol, New York, NY USA.
[Sofge, Don] Naval Res Lab, Washington, DC USA.
[Lawless, William] Pain Coll, Augusta, GA USA.
[Sridharan, Mohan] Texas Tech Univ, Lubbock, TX 79409 USA.
[Hawes, Nick] Univ Birmingham, Sch Comp Sci, Birmingham B15 2TT, W Midlands, England.
[Hwang, Tim] Pacific Social Architecting Corp, New York, NY USA.
[Hwang, Tim] Data & Soc Res Inst New York City, New York, NY USA.
RP Jain, M (reprint author), Virginia Polytech Inst & State Univ, Dept Comp Sci, Blacksburg, VA 24061 USA.
OI Hawes, Nick/0000-0002-7556-6098
NR 0
TC 0
Z9 0
U1 1
U2 6
PU AMER ASSOC ARTIFICIAL INTELL
PI MENLO PK
PA 445 BURGESS DRIVE, MENLO PK, CA 94025-3496 USA
SN 0738-4602
J9 AI MAG
JI AI Mag.
PD FAL
PY 2014
VL 35
IS 3
BP 70
EP 76
PG 7
WC Computer Science, Artificial Intelligence
SC Computer Science
GA AP1DB
UT WOS:000341805500008
ER
PT J
AU Anenberg, SC
West, JJ
Yu, HB
Chin, M
Schulz, M
Bergmann, D
Bey, I
Bian, HS
Diehl, T
Fiore, A
Hess, P
Marmer, E
Montanaro, V
Park, R
Shindell, D
Takemura, T
Dentener, F
AF Anenberg, Susan C.
West, J. Jason
Yu, Hongbin
Chin, Mian
Schulz, Michael
Bergmann, Dan
Bey, Isabelle
Bian, Huisheng
Diehl, Thomas
Fiore, Arlene
Hess, Peter
Marmer, Elina
Montanaro, Veronica
Park, Rokjin
Shindell, Drew
Takemura, Toshihiko
Dentener, Frank
TI Impacts of intercontinental transport of anthropogenic fine particulate
matter on human mortality
SO AIR QUALITY ATMOSPHERE AND HEALTH
LA English
DT Article
DE Health impact assessment; Particulate matter; Long-range transport;
Chemical transport modeling
ID REGIONAL AIR-QUALITY; MULTIMODEL ASSESSMENT; EMISSION CONTROLS; GLOBAL
BURDEN; UNITED-STATES; POLLUTION; AEROSOL; OZONE; EXPOSURE; VISIBILITY
AB Fine particulate matter with diameter of 2.5 mu m or less (PM2.5) is associated with premature mortality and can travel long distances, impacting air quality and health on intercontinental scales. We estimate the mortality impacts of 20 % anthropogenic primary PM2.5 and PM2.5 precursor emission reductions in each of four major industrial regions (North America, Europe, East Asia, and South Asia) using an ensemble of global chemical transport model simulations coordinated by the Task Force on Hemispheric Transport of Air Pollution and epidemiologically-derived concentration-response functions. We estimate that while 93-97 % of avoided deaths from reducing emissions in all four regions occur within the source region, 3-7 % (11,500; 95 % confidence interval, 8,800-14,200) occur outside the source region from concentrations transported between continents. Approximately 17 and 13 % of global deaths avoided by reducing North America and Europe emissions occur extraregionally, owing to large downwind populations, compared with 4 and 2 % for South and East Asia. The coarse resolution global models used here may underestimate intraregional health benefits occurring on local scales, affecting these relative contributions of extraregional versus intraregional health benefits. Compared with a previous study of 20 % ozone precursor emission reductions, we find that despite greater transport efficiency for ozone, absolute mortality impacts of intercontinental PM2.5 transport are comparable or greater for neighboring source-receptor pairs, due to the stronger effect of PM2.5 on mortality. However, uncertainties in modeling and concentration-response relationships are large for both estimates.
C1 [Anenberg, Susan C.] US EPA, Washington, DC 20460 USA.
[West, J. Jason] Univ N Carolina, Chapel Hill, NC USA.
[Yu, Hongbin] Univ Maryland, College Pk, MD 20742 USA.
[Chin, Mian; Bian, Huisheng; Diehl, Thomas] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Schulz, Michael] Norwegian Meteorol Inst, Oslo, Norway.
[Bergmann, Dan] Lawrence Livermore Natl Lab, Livermore, CA USA.
[Bey, Isabelle] Swiss Fed Inst Technol, Zurich, Switzerland.
[Diehl, Thomas] Univ Space Res Assoc, Columbia, MD USA.
[Fiore, Arlene] Columbia Univ, Lamont Doherty Geol Observ, Palisades, NY 10964 USA.
[Hess, Peter] Cornell Univ, Dept Biol & Environm Engn, Ithaca, NY USA.
[Marmer, Elina] Univ Hamburg, Dept Educ, Hamburg, Germany.
[Montanaro, Veronica] Univ Aquila, I-67100 Laquila, Italy.
[Park, Rokjin] Seoul Natl Univ, Seoul, South Korea.
[Shindell, Drew] NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
[Shindell, Drew] Columbia Earth Inst, New York, NY USA.
[Takemura, Toshihiko] Kyushu Univ, Appl Mech Res Inst, Fukuoka 8168580, Japan.
[Dentener, Frank] Commiss European Communities, Joint Res Ctr, Inst Environm & Sustainabil, I-21020 Ispra, Italy.
RP Anenberg, SC (reprint author), US EPA, 1200 Penn Ave NW MC6301A, Washington, DC 20460 USA.
EM anenberg.susan@epa.gov
RI Yu, Hongbin/C-6485-2008; Takemura, Toshihiko/C-2822-2009; Kyushu,
RIAM/F-4018-2015; West, Jason/J-2322-2015; Park, Rokjin/I-5055-2012;
Shindell, Drew/D-4636-2012; Schulz, Michael/A-6930-2011; U-ID,
Kyushu/C-5291-2016; Chin, Mian/J-8354-2012
OI Yu, Hongbin/0000-0003-4706-1575; Takemura,
Toshihiko/0000-0002-2859-6067; West, Jason/0000-0001-5652-4987; Park,
Rokjin/0000-0001-8922-0234; Schulz, Michael/0000-0003-4493-4158;
FU NASA; US Department of Energy (BER) at LLNL [DE-AC5207NA27344]
FX The opinions expressed in this article are the authors' and do not
necessarily represent those of their employers, including the USEPA.
Model simulations were performed under the UN ECE Task Force on
Hemispheric Transport of Air Pollution. H. Y. was supported by the NASA
Atmospheric Composition Modeling and Analysis Program administered by R.
Eckman. D. B. was supported by the US Department of Energy (BER) at LLNL
under contract DE-AC5207NA27344.
NR 48
TC 6
Z9 6
U1 7
U2 40
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 SEP
PY 2014
VL 7
IS 3
BP 369
EP 379
DI 10.1007/s11869-014-0248-9
PG 11
WC Environmental Sciences
SC Environmental Sciences & Ecology
GA AO8GP
UT WOS:000341592100011
ER
PT J
AU Hasoglu, MF
Abdel-Naby, SA
Gatuzz, E
Garcia, J
Kallman, TR
Mendoza, C
Gorczyca, TW
AF Hasoglu, M. F.
Abdel-Naby, Sh. A.
Gatuzz, E.
Garcia, J.
Kallman, T. R.
Mendoza, C.
Gorczyca, T. W.
TI K-SHELL PHOTOABSORPTION OF MAGNESIUM IONS
SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES
LA English
DT Article
DE atomic data; atomic processes; ISM: abundances; line: formation
ID X-RAY SPECTROSCOPY; PHOTOIONIZATION CROSS-SECTIONS; XMM-NEWTON
OBSERVATION; INTERSTELLAR-MEDIUM; FLUORESCENCE YIELDS; ATOMIC OXYGEN;
ABSORPTION; CHANDRA; AUGER; ABUNDANCES
AB X-ray photoabsorption cross sections have been computed for all magnesium ions with three or more electrons using the R-matrix method. A comparison with other available data for Mg II-Mg x shows good qualitative agreement in the resultant resonance shapes. However, for the lower ionization stages, and for singly ionized Mg II in particular, the previous R-matrix results overestimate the K-edge position due to the neglect of important orbital relaxation effects, and a global shift downward in photon energy of those cross sections is therefore warranted. We have found that the cross sections for Mg I and Mg II are further complicated by the M-shell (n = 3) occupancy. As a result, the treatment of spectator Auger decay of 1s -> np resonances using a method based on multichannel quantum defect theory and an optical potential becomes problematic, making it necessary to implement an alternative, approximate treatment of Auger decay for neutral Mg I. The new cross sections are used to fit the Mg K edge in XMM-Newton spectra of the low-mass X-ray binary GS 1826-238, where most of the interstellar Mg is found to be in ionized form.
C1 [Hasoglu, M. F.] Hasan Kalyoncu Univ, Dept Comp Engn, TR-27100 Sahinbey, Gaziantep, Turkey.
[Abdel-Naby, Sh. A.] Auburn Univ, Dept Phys, Auburn, AL 36849 USA.
[Gatuzz, E.; Mendoza, C.] Inst Venezolano Invest Cient, Ctr Fis, Caracas 1020, Venezuela.
[Garcia, J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Kallman, T. R.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Mendoza, C.; Gorczyca, T. W.] Western Michigan Univ, Dept Phys, Kalamazoo, MI 49008 USA.
RP Hasoglu, MF (reprint author), Hasan Kalyoncu Univ, Dept Comp Engn, TR-27100 Sahinbey, Gaziantep, Turkey.
OI Mendoza, Claudio/0000-0002-2854-4806
FU NASA APRA grant [NNX11AF32G]
FX This work was supported in part by the NASA APRA grant NNX11AF32G.
NR 55
TC 3
Z9 3
U1 1
U2 7
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0067-0049
EI 1538-4365
J9 ASTROPHYS J SUPPL S
JI Astrophys. J. Suppl. Ser.
PD SEP
PY 2014
VL 214
IS 1
AR 8
DI 10.1088/0067-0049/214/1/8
PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AP0TP
UT WOS:000341777800008
ER
PT J
AU Gopalswamy, N
Xie, H
Akiyama, S
Makela, PA
Yashiro, S
AF Gopalswamy, Nat
Xie, Hong
Akiyama, Sachiko
Makela, Pertti A.
Yashiro, Seiji
TI Major solar eruptions and high-energy particle events during solar cycle
24
SO EARTH PLANETS AND SPACE
LA English
DT Article
DE Coronal mass ejections; Flares; Ground level enhancement events; Solar
energetic particle events
ID CORONAL MASS EJECTIONS; II RADIO-BURSTS; GROUND-LEVEL ENHANCEMENT; SPACE
WEATHER; PROTON EVENTS; PEAK INTENSITIES; SHOCK FORMATION; NEAR-SUN;
VARIABILITY; FLARES
AB We report on a study of all major solar eruptions that occurred on the frontside of the Sun during the rise to peak phase of cycle 24 (first 62 months) in order to understand the key factors affecting the occurrence of large solar energetic particle events (SEPs) and ground level enhancement (GLE) events. The eruptions involve major flares with soft X-ray peak flux >= 5.0 x 10(-5) Wm(-2) (i.e., flare size >= M5.0) and accompanying coronal mass ejections (CMEs). The selection criterion was based on the fact that the only front-side GLE in cycle 24 (GLE 71) had a flare size of M5.1. Only approximately 37% of the major eruptions from the western hemisphere resulted in large SEP events. Almost the same number of large SEP events was produced in weaker eruptions (flare size < M5.0), suggesting that the soft X-ray flare is not a good indicator of SEP or GLE events. On the other hand, the CME speed is a good indicator of SEP and GLE events because it is consistently high supporting the shock acceleration mechanism. We found the CME speed, magnetic connectivity to Earth (in longitude and latitude), and ambient conditions as the main factors that contribute to the lack of high-energy particle events during cycle 24. Several eruptions poorly connected to Earth (eastern-hemisphere or behind-the-west-limb events) resulted in very large SEP events detected by the Solar Terrestrial Relations Observatory (STEREO) spacecraft. Some very fast CMEs, likely to have accelerated particles to GeV energies, did not result in a GLE event because of poor latitudinal connectivity. The stringent latitudinal requirement suggests that the highest-energy particles are likely accelerated in the nose part of shocks, while the lower energy particles are accelerated at all parts. There were also well-connected fast CMEs, which did not seem to have accelerated high-energy particles due to possible unfavorable ambient conditions (high Alfven speed, overall reduction in acceleration efficiency in cycle 24).
C1 [Gopalswamy, Nat] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Xie, Hong; Akiyama, Sachiko; Makela, Pertti A.; Yashiro, Seiji] Catholic Univ Amer, Washington, DC 20064 USA.
RP Gopalswamy, N (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
EM nat.gopalswamy@nasa.gov
OI Gopalswamy, Nat/0000-0001-5894-9954
FU NASA's LWS; LWS TRT
FX This work was supported by NASA's LWS and LWS TR&T programs. This work
benefitted greatly from the open data policy of NASA.
NR 48
TC 20
Z9 20
U1 2
U2 7
PU SPRINGER HEIDELBERG
PI HEIDELBERG
PA TIERGARTENSTRASSE 17, D-69121 HEIDELBERG, GERMANY
SN 1880-5981
J9 EARTH PLANETS SPACE
JI Earth Planets Space
PD SEP 1
PY 2014
VL 66
AR 104
DI 10.1186/1880-5981-66-104
PG 15
WC Geosciences, Multidisciplinary
SC Geology
GA AP6EG
UT WOS:000342169800001
ER
PT J
AU Cartwright, JA
Ott, U
Mittlefehldt, DW
AF Cartwright, J. A.
Ott, U.
Mittlefehldt, D. W.
TI The quest for regolithic howardites. Part 2: Surface origins highlighted
by noble gases
SO GEOCHIMICA ET COSMOCHIMICA ACTA
LA English
DT Article
ID CALCIUM-RICH ACHONDRITES; CARBONACEOUS CHONDRITE CLASTS; ANCIENT
SOLAR-ACTIVITY; PARENT BODY REGOLITH; RAY EXPOSURE AGES; ANGRA-DOS-REIS;
BASALTIC ACHONDRITES; ANTARCTIC METEORITES; PRODUCTION-RATES; COSMOGENIC
NEON
AB We report noble gas data of helium (He), neon (Ne), argon (Ar), krypton (Kr) and xenon (Xe), cosmic ray exposure (CRE) ages and nominal gas retention (K Ar, U Th He) ages for seven howardites (CRE 01400, EET 87513, EET 87518, EET 99400, GRO 95535, GRO 95602, SAN 03472), in continuing research to identify regolithic samples, and better understand the vestan regolith. In our previous work, we found little correlation between suggested regolith parameters of Ni > 300 mu g/g, Al2O3 8-9 wt% and eucrite/diogenite (E:D) ratio of 2:1 (Warren et al., 2009), and trapped solar wind (SW), fractionated solar wind (FSW) or planetary noble gas components (from impacted material) -noble gas indicators of a regolithic origin. Here, we have expanded our data set to include samples outside of these parameters to further explore composition, and the differences in Ni content as indicators for the presence of non-Vesta material. In addition, our sample set includes two potentially paired meteorites from the GRO suite. Finally, in our petrographic studies, the samples selected showed no evidence for carbonaceous chondrite fragments, which should reduce the effect of "contamination" by planetary noble gas components, and will allow us to better identify SW/FSW components, where present.
Of the samples studied here, three howardites GRO 95535, GRO 95602 and EET 87513 show evidence for a regolithic origin, with both isotopic and element noble gas ratios clearly pointing to the presence of trapped components similar to SW/FSW or planetary. The two GRO howardites, GRO 95535 and GRO 95602, show similar noble gas ratios to our previously defined SW/FSW dominated regolithic group (LEW 85313 and MET 00423), suggesting a surface origin for these samples. However, interestingly, the GRO samples show vastly different cosmogenic noble gas abundances, and thus different CRE ages, which suggests that they are not paired. For howardite EET 87513, the data hint to the presence of CM-material, with a neon release pattern similar to our defined planetary/FSW dominated regolithic group (CM-rich samples PRA 04401, SCO 06040). Our petrological investigations found no evidence for CM fragments within EET 87513, though a single clast was reported previously (Buchanan et al., 1993). Aside from the Ne release pattern, the remaining noble gas data show more similarity with SW/FSW components. The remaining four howardites CRE 01400, EET 87518, EET 99400, and SAN 03472 and are dominated by cosmogenic noble gases, and show no evidence for a regolithic origin. Our data suggest that a CM-composition is likely present in all samples to some degree, but that this can be overprinted by SW components or cosmogenic components obtained in situ on the vestan surface or during transit to Earth respectively.
The presence of CM material is an important parameter for understanding the evolution of Vesta's surface. While we have uncovered three further regolithic howardites (similar to 13 regolithic total, of similar to 41 analysed), further noble gas analysis of HED meteorites is needed to not only determine regolithic origins, but to better characterise the abundance of carbonaceous chondrite material and its effect on the noble gas signatures of such samples. (C) 2014 Elsevier Ltd. All rights reserved.
C1 [Cartwright, J. A.; Ott, U.] Max Planck Inst Chem, D-55128 Mainz, Germany.
[Cartwright, J. A.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA.
[Ott, U.] Univ West Hungary, H-9700 Szombathely, Hungary.
[Mittlefehldt, D. W.] NASA, Lyndon B Johnson Space Ctr, Astromat Res Off, Houston, TX 77058 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
FU National Science Foundation (USA)
FX We thank the National Science Foundation (USA) 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.
NR 111
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Z9 8
U1 3
U2 13
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 SEP 1
PY 2014
VL 140
BP 488
EP 508
DI 10.1016/j.gca.2014.05.033
PG 21
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA AP2SP
UT WOS:000341925300031
ER
PT J
AU Feuerecker, M
Crucian, B
Salam, AP
Rybka, A
Kaufmann, I
Moreels, M
Quintens, R
Schelling, G
Thiel, M
Baatout, S
Sams, C
Chouker, A
AF Feuerecker, Matthias
Crucian, Brian
Salam, Alex P.
Rybka, Ales
Kaufmann, Ines
Moreels, Marjan
Quintens, Roel
Schelling, Gustav
Thiel, Manfred
Baatout, Sarah
Sams, Clarence
Chouker, Alexander
TI Early Adaption to the Antarctic Environment at Dome C: Consequences on
Stress-Sensitive Innate Immune Functions
SO HIGH ALTITUDE MEDICINE & BIOLOGY
LA English
DT Article
DE adenosine; Antarctica; hormones; hypobaric hypoxia; polymorphonuclear
leukocytes (PMNs)
ID ADENOSINE A(2A) RECEPTORS; HIGH-ALTITUDE; HEALTHY-VOLUNTEERS; HYPOXIA;
CORTISOL; MEGAKARYOCYTOPOIESIS; CATECHOLAMINES; INFLAMMATION; RESPONSES;
AFFINITY
AB Purpose/Aims: Medical reports of Antarctic expeditions indicate that health is affected under these extreme conditions. The present study at CONCORDIA-Station (Dome C, 3233 m) seeks to investigate the early consequences of confinement and hypobaric hypoxia on the human organism. Methods: Nine healthy male participants were included in this study. Data collection occurred before traveling to Antarctica (baseline), and at 1 week and 1 month upon arrival. Investigated parameters included basic physiological variables, psychological stress tests, cell blood count, stress hormones, and markers of innate immune functions in resting and stimulated immune cells. By testing for the hydrogen peroxide (H2O2) production of stimulated polymorphonuclear leukocytes (PMNs), the effects of the hypoxia-adenosine-sensitive immune modulatory pathways were examined. Results: As compared to baseline data, reduced oxygen saturation, hemoconcentration, and an increase of secreted catecholamines was observed, whereas no psychological stress was seen. Upon stimulation, the activity of PMNs and L-selectin shedding was mitigated after 1 week. Endogenous adenosine concentration was elevated during the early phase. In summary, living conditions at high altitude influence the innate immune system's response. After 1 month, some of the early effects on the human organism were restored. Conclusion: As this early adaptation is not related to psychological stress, the changes observed are likely to be induced by environmental stressors, especially hypoxia. As hypoxia is triggering ATP-catabolism, leading to elevated endogenous adenosine concentrations, this and the increased catecholamine concentration might contribute to the early, but reversible downregulation of innate immune functions. This indicates the slope of innate immune adaptation to hypoxia.
C1 [Feuerecker, Matthias; Kaufmann, Ines; Schelling, Gustav; Chouker, Alexander] Univ Munich, Dept Anaesthesiol, Klinikum Grosshadern, Res Grp Stress & Immun, D-81377 Munich, Germany.
[Crucian, Brian; Sams, Clarence] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA.
[Salam, Alex P.; Rybka, Ales] European Space Agcy, Concordia, Dome, France.
[Salam, Alex P.] Univ Oxford, Inst Cognit & Evolutionary Anthropol, London, England.
[Moreels, Marjan; Quintens, Roel; Baatout, Sarah] CEN SCK, Belgian Nucl Res Ctr, Radiobiol Unit, B-2400 Mol, Belgium.
[Thiel, Manfred] Heidelberg Univ, Fac Med, Dept Anaesthesiol & Intens Care, Mannheim, Germany.
[Baatout, Sarah] Univ Ghent, Dept Mol Biotechnol, Ghent, Belgium.
RP Chouker, A (reprint author), Univ Munich, Dept Anaesthesiol, Marchioninistr 15, D-81377 Munich, Germany.
EM alexander.chouker@med.uni-muenchen.de
FU European Space Agency; French (IPEV) polar institute; Italian (PNRA)
polar institute; German National Space Program (DLR) [50WB0719/WB0919];
2 PRODEX/BELSPO/ESA [C90-391, 42-000-90-380]; NASA (JSC)
FX The authors are grateful to the support from the European Space Agency
(ESA ELIPS 3 and 4 programs), the French (IPEV) and Italian (PNRA) polar
institutes, and the German National Space Program (DLR,
50WB0719/WB0919). This research was also financially supported by the 2
PRODEX/BELSPO/ESA contracts (C90-391 and 42-000-90-380) and NASA (JSC).
NR 37
TC 2
Z9 4
U1 2
U2 12
PU MARY ANN LIEBERT, INC
PI NEW ROCHELLE
PA 140 HUGUENOT STREET, 3RD FL, NEW ROCHELLE, NY 10801 USA
SN 1527-0297
EI 1557-8682
J9 HIGH ALT MED BIOL
JI High Alt. Med. Biol.
PD SEP
PY 2014
VL 15
IS 3
BP 341
EP 348
DI 10.1089/ham.2013.1128
PG 8
WC Biophysics; Public, Environmental & Occupational Health; Sport Sciences
SC Biophysics; Public, Environmental & Occupational Health; Sport Sciences
GA AP5ZL
UT WOS:000342157100009
PM 25099674
ER
PT J
AU Mukhanov, O
Prokopenko, G
Romanofsky, R
AF Mukhanov, Oleg
Prokopenko, Georgy
Romanofsky, Robert
TI Quantum Sensitivity
SO IEEE MICROWAVE MAGAZINE
LA English
DT Article
ID INTERFERENCE FILTERS; MAGNETIC-FIELD; MAGNETOMETERS; SYSTEMS; RADIO
C1 [Mukhanov, Oleg; Prokopenko, Georgy] Hypres Inc, Elmsford, NY 10523 USA.
[Romanofsky, Robert] NASA, Glenn Res Ctr, Cleveland, OH USA.
RP Mukhanov, O (reprint author), Hypres Inc, 175 Clearbrook Rd, Elmsford, NY 10523 USA.
EM mukhanov@hypres.com
NR 38
TC 11
Z9 11
U1 0
U2 4
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 1527-3342
EI 1557-9581
J9 IEEE MICROW MAG
JI IEEE Microw. Mag.
PD SEP-OCT
PY 2014
VL 15
IS 6
BP 57
EP 65
DI 10.1109/MMM.2014.2332421
PG 9
WC Engineering, Electrical & Electronic; Telecommunications
SC Engineering; Telecommunications
GA AP4UX
UT WOS:000342075400008
ER
PT J
AU Scaramuzza, D
Achtelik, MC
Doitsidis, L
Fraundorfer, F
Kosmatopoulos, E
Martinelli, A
Achtelik, MW
Chli, M
Chatzichristofis, S
Kneip, L
Gurdan, D
Heng, L
Lee, GH
Lynen, S
Meier, L
Pollefeys, M
Renzaglia, A
Siegwart, R
Stumpf, JC
Tanskanen, P
Troiani, C
Weiss, S
AF Scaramuzza, Davide
Achtelik, Michael C.
Doitsidis, Lefteris
Fraundorfer, Friedrich
Kosmatopoulos, Elias
Martinelli, Agostino
Achtelik, Markus W.
Chli, Margarita
Chatzichristofis, Savvas
Kneip, Laurent
Gurdan, Daniel
Heng, Lionel
Lee, Gim Hee
Lynen, Simon
Meier, Lorenz
Pollefeys, Marc
Renzaglia, Alessandro
Siegwart, Roland
Stumpf, Jan Carsten
Tanskanen, Petri
Troiani, Chiara
Weiss, Stephan
TI Vision-Controlled Micro Flying Robots From System Design to Autonomous
Navigation and Mapping in GPS-Denied Environments
SO IEEE ROBOTICS & AUTOMATION MAGAZINE
LA English
DT Article
ID OPTIMIZATION; ALGORITHMS; QUADROTOR; COVERAGE; SCALE
C1 [Scaramuzza, Davide] Univ Zurich, CH-8050 Zurich, Switzerland.
[Achtelik, Michael C.; Gurdan, Daniel; Stumpf, Jan Carsten] Ascending Technol GmbH, D-82152 Krailling, Germany.
[Doitsidis, Lefteris] Technol Educ Inst Crete, Khania 73100, Greece.
[Fraundorfer, Friedrich] Tech Univ Munich, D-80333 Munich, Germany.
[Kosmatopoulos, Elias; Chatzichristofis, Savvas] Democritus Univ Thrace, GR-67100 Xanthi, Greece.
[Kosmatopoulos, Elias; Chatzichristofis, Savvas] ITI CERTH, Xanthi 67100, Greece.
[Martinelli, Agostino] INRIA Grenoble Rhone Alpes, F-38334 Grenoble, France.
[Achtelik, Markus W.] ETH, Autonomous Syst Lab, CH-8092 Zurich, Switzerland.
[Chli, Margarita] Univ Edinburgh, Edinburgh EH8 9AB, Midlothian, Scotland.
[Kneip, Laurent] Australian Natl Univ, Canberra, ACT 0200, Australia.
[Heng, Lionel; Lynen, Simon; Meier, Lorenz; Siegwart, Roland; Tanskanen, Petri] ETH, CH-8092 Zurich, Switzerland.
[Lee, Gim Hee] ETH, CH-8051 Zurich, Switzerland.
[Pollefeys, Marc] ETH, CH-8006 Zurich, Switzerland.
[Renzaglia, Alessandro] Univ Minnesota, Minneapolis, MN 55455 USA.
[Troiani, Chiara] INRIA Rhone Alpes, F-38334 Grenoble, France.
[Weiss, Stephan] NASA Jet Prop Lab, Pasadena, CA 91109 USA.
[Weiss, Stephan] CALTECH, Pasadena, CA 91109 USA.
RP Scaramuzza, D (reprint author), Univ Zurich, CH-8050 Zurich, Switzerland.
EM davide.scaramuzza@ieee.org; michael@achtelik.net;
ldoitsidis@chania.teicrete.gr; friedrich.fraundorfer@tum.de;
kosmatop@dssl.tuc.gr; agostino.martinelli@inria.fr;
markus.achtelik@mavt.ethz.ch; margarita.chli@mavt.ethz.ch;
schatzic@ee.duth.gr; laurent.kneip@anu.edu.au; daniel@gurdan.de;
hengli@inf.ethz.ch; lgimhee@gmail.com; simon.lynen@mavt.ethz.ch;
lm@inf.ethz.ch; marc.pollefeys@inf.ethz.ch; a.renzaglia@gmail.com;
rsiegwart@ethz.ch; jan@asctec.de; tpetri@student.ethz.ch;
chiara.troiani@inrialpes.fr; stephan.weiss@ieee.org
RI Lee, Gim Hee/K-5241-2015;
OI Kneip, Laurent/0000-0001-6727-6608
NR 58
TC 35
Z9 35
U1 5
U2 50
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 1070-9932
EI 1558-223X
J9 IEEE ROBOT AUTOM MAG
JI IEEE Robot. Autom. Mag.
PD SEP
PY 2014
VL 21
IS 3
BP 26
EP 40
DI 10.1109/MRA.2014.2322295
PG 15
WC Automation & Control Systems; Robotics
SC Automation & Control Systems; Robotics
GA AP4YW
UT WOS:000342087700007
ER
PT J
AU Giangrande, SE
Collis, S
Theisen, AK
Tokay, A
AF Giangrande, Scott E.
Collis, Scott
Theisen, Adam K.
Tokay, Ali
TI Precipitation Estimation from the ARM Distributed Radar Network during
the MC3E Campaign
SO JOURNAL OF APPLIED METEOROLOGY AND CLIMATOLOGY
LA English
DT Article
ID MESOSCALE CONVECTIVE SYSTEMS; DUAL-POLARIZATION RADAR; X-BAND;
DIFFERENTIAL PHASE; C-BAND; RAINFALL ESTIMATION; POLARIMETRIC RADAR;
WEATHER RADAR; ERROR VARIANCE; PART II
AB This study presents radar-based precipitation estimates collected during the 2-month U. S. Department of Energy Atmospheric Radiation Measurement Program (ARM)-NASA Midlatitude Continental Convective Clouds Experiment (MC3E). Emphasis is on the usefulness of radar observations from the C-band and X-band scanning ARM precipitation radars (CSAPR and XSAPR, respectively) for rainfall estimation products to distances within 100 km of the Lamont, Oklahoma, ARM facility. The study utilizes a dense collection of collocated ARM, NASA Global Precipitation Measurement, and nearby surface Oklahoma Mesonet gauge records to evaluate radar-based hourly rainfall products and campaign-optimized methods over individual gauges and for areal rainfall characterizations. Rainfall products are also evaluated against the performance of a regional NWS Weather Surveillance Radar-1988 Doppler (WSR-88D) S-band dual-polarization radar product. Results indicate that the CSAPR system may achieve similar point-and areal-gauge bias and root-mean-square (RMS) error performance to a WSR-88D reference for the variety of MC3E deep convective events sampled. The best campaign rainfall performance was achieved when using radar relations capitalizing on estimates of the specific attenuation from the CSAPR system. The XSAPRs demonstrate limited capabilities, having modest success in comparison with the WSR-88D reference for hourly rainfall accumulations that are under 10mm. All rainfall estimation methods exhibit a reduction by a factor of 1.5-2.5 in RMS errors for areal accumulations over a 15-km(2) NASA dense gauge network, with the smallest errors typically associated with dual-polarization radar methods.
C1 [Giangrande, Scott E.] Brookhaven Natl Lab, Div Atmospher Sci, Upton, NY 11973 USA.
[Collis, Scott] Argonne Natl Lab, Div Environm Sci, Argonne, IL 60439 USA.
[Theisen, Adam K.] Univ Oklahoma, Cooperat Inst Mesoscale Meteorol Studies, Atmospher Radiat Measurement Program, Data Qual Off, Norman, OK 73019 USA.
[Tokay, Ali] Univ Maryland Baltimore Cty, Baltimore, MD 21228 USA.
[Tokay, Ali] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Giangrande, SE (reprint author), Brookhaven Natl Lab, Div Atmospher Sci, Bldg 490D,Bell Ave, Upton, NY 11973 USA.
EM scott.giangrande@bnl.gov
RI Measurement, Global/C-4698-2015; Giangrande, Scott/I-4089-2016
OI Giangrande, Scott/0000-0002-8119-8199
FU Brookhaven Science Associates, LLC [DE-AC02-98CH10886]; U.S. Department
of Energy; Climate Science for a Sustainable Energy Future (CSSEF)
project of the Earth System Modeling (ESM) program in the DOE Office of
Science; U.S. Department of Energy Office of Science, Office of
Biological and Environmental Research (OBER) [DE-AC02-06CH11357]; OBER
of the DOE as part of the ARM Program; Battelle-Pacific Northwest
National Laboratory [206248]; NOAA/Office of Oceanic and Atmospheric
Research under U.S. Department of Commerce NOAA-University of Oklahoma
[NA11OAR4320072]
FX This paper has been authored by employees of Brookhaven Science
Associates, LLC, under Contract DE-AC02-98CH10886 with the U.S.
Department of Energy. The publisher by accepting the paper for
publication acknowledges that the U.S. government retains a
nonexclusive, paid-up, irrevocable, worldwide license to publish or
reproduce the published form of this paper, or to allow others to do so,
for U.S. government purposes. Author Giangrande's work is supported by
the Climate Science for a Sustainable Energy Future (CSSEF) project of
the Earth System Modeling (ESM) program in the DOE Office of Science.
Argonne National Laboratory's work was supported by the U.S. Department
of Energy Office of Science, Office of Biological and Environmental
Research (OBER), under Contract DE-AC02-06CH11357. The work has been
supported by the OBER of the DOE as part of the ARM Program. Adam
Theisen's work was supported by Battelle-Pacific Northwest National
Laboratory, Contract 206248, and his home institution CIMMS is supported
by NOAA/Office of Oceanic and Atmospheric Research under U.S. Department
of Commerce NOAA-University of Oklahoma Cooperative Agreement
NA11OAR4320072. The authors thank Dr. Alexander Ryzhkov for support on
implementation of specific-attenuation-based rainfall methods,
associated comments, and considerations. We thank Michael Jensen of BNL,
Virendra Ghate of ANL, and Randy Peppler of OU-CIMMS for internal
reviews of this manuscript.
NR 63
TC 9
Z9 9
U1 1
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 SEP
PY 2014
VL 53
IS 9
BP 2130
EP 2147
DI 10.1175/JAMC-D-13-0321.1
PG 18
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA AP3ZY
UT WOS:000342017800003
ER
PT J
AU Shuman, CA
Hall, DK
DiGirolamo, NE
Mefford, TK
Schnaubelt, MJ
AF Shuman, Christopher A.
Hall, Dorothy K.
DiGirolamo, Nicolo E.
Mefford, Thomas K.
Schnaubelt, Michael J.
TI Comparison of Near-Surface Air Temperatures and MODIS Ice-Surface
Temperatures at Summit, Greenland (2008-13)
SO JOURNAL OF APPLIED METEOROLOGY AND CLIMATOLOGY
LA English
DT Article
ID POLAR PATHFINDER DATASET; CLOUD DETECTION; ANTARCTIC PLATEAU; ARCTIC
SURFACE; ABLATION ZONE; PART II; SHEET; MELT; SATELLITE; CLIMATE
AB The stability of the Moderate Resolution Imaging Spectroradiometer (MODIS) ice-surface temperature (IST) product from Terra was investigated for use as a climate-quality data record. The availability of climate-quality air temperature data T-A from a NOAA observatory at Greenland's Summit Station has enabled this high-temporal-resolution study of MODIS ISTs. During a > 5-yr period (July 2008-August 2013), more than 2500 IST values were compared with +/- 3-min-average T-A values from NOAA's primary 2-m temperature sensor. This enabled an expected small offset between air and ice-sheet surface temperatures (T-A > IST) to be investigated over multiple annual cycles. The principal findings of this study show 1) that IST values are slightly colder than the T-A values near freezing but that this offset increases as temperature decreases and 2) that there is a pattern in IST-T-A differences as the solar zenith angle (SoZA) varies annually. This latter result largely explains the progressive offset from the in situ data at colder temperatures but also indicates that the MODIS cloud mask is less accurate approaching and during the polar night. The consistency of the results over each year in this study indicates that MODIS provides a platform for remotely deriving surface temperature data, with the resulting IST data being most compatible with in situ T-A data when the sky is clear and the SoZA is less than similar to 85 degrees. The ongoing development of the IST dataset should benefit from improved cloud filtering as well as algorithm modifications to account for the progressive offset from T-A at colder temperatures.
C1 [Shuman, Christopher A.; Schnaubelt, Michael J.] Univ Maryland Baltimore Cty, Joint Ctr Earth Syst Technol, Greenbelt, MD 20771 USA.
[Shuman, Christopher A.; DiGirolamo, Nicolo E.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Hall, Dorothy K.] NASA, Goddard Space Flight Ctr, Cryospher Sci Lab, Greenbelt, MD 20771 USA.
[DiGirolamo, Nicolo E.] Sci Syst & Applicat Inc, Greenbelt, MD USA.
[Mefford, Thomas K.] Univ Colorado, Cooperat Inst Res Environm Sci, Boulder, CO 80309 USA.
[Mefford, Thomas K.] NOAA, Earth Syst Res Lab, Boulder, CO USA.
RP Shuman, CA (reprint author), Univ Maryland Baltimore Cty, Joint Ctr Earth Syst Technol, Code 615, Greenbelt, MD 20771 USA.
EM christopher.a.shuman@nasa.gov
FU NASA's Cryospheric Sciences Program
FX The authors thank the support staff at the Greenland Summit Station for
helping to provide the in situ data necessary for this study. The TA
data were derived from NOAA's Earth System Research Laboratory Global
Monitoring Division datasets. NASA's Cryospheric Sciences Program
provided funding for the MODIS IST dataset as well as the work performed
at NASA Goddard Space Flight Center (GSFC) and at University of
Maryland, Baltimore County. Jack Xiong and Brian Wenny of the MODIS
Characterization and Support Team at GSFC and George Riggs (Science
Systems and Applications, Inc., at GSFC), provided additional insights
on the IST data and MODIS products. We thank the editor and three
anonymous reviewers for their comments and guidance that improved the
final paper.
NR 39
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U1 1
U2 10
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 SEP
PY 2014
VL 53
IS 9
BP 2171
EP 2180
DI 10.1175/JAMC-D-14-0023.1
PG 10
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA AP3ZY
UT WOS:000342017800006
ER
PT J
AU Kelley, OA
AF Kelley, Owen A.
TI Where the Least Rainfall Occurs in the Sahara Desert, the TRMM Radar
Reveals a Different Pattern of Rainfall Each Season
SO JOURNAL OF CLIMATE
LA English
DT Article
ID WEST-AFRICA; PRECIPITATION RADAR; CLIMATE-CHANGE; LAND-SURFACE;
VARIABILITY; SATELLITE; MODEL; SYSTEMS; OCEAN; CLASSIFICATION
AB Some previous studies were unable to detect seasonal organization to the rainfall in the Sahara Desert, while others reported seasonal patterns only in the less-arid periphery of the Sahara. In contrast, the precipitation radar on the Tropical Rainfall Measuring Mission (TRMM) satellite detects four rainy seasons in the part of the Sahara where the TRMM radar saw the least rainfall during a 15-yr period (1998-2012). According to the TRMM radar, approximately 20 degrees-27 degrees N, 22 degrees-32 degrees E is the portion of the Sahara that has the lowest average annual rain accumulation (1-5 mm yr(-1)). Winter (January and February) has light rain throughout this region but more rain to the north over the Mediterranean Sea. Spring (April and May) has heavier rain and has lightning observed by the TRMM Lightning Imaging Sensor (LIS). Summer rain and lightning (July and August) occur primarily south of 23 degrees N. At a maximum over the Red Sea, autumn rain and lightning (October and November) can be heavy in the northeastern portion of the study area, but these storms are unreliable: that is, the TRMM radar detects such storms in only 6 of the 15 years. These four rainy seasons are each separated by a comparatively drier month in the monthly rainfall climatology. The few rain gauges in this arid region broadly agree with the TRMM radar on the seasonal organization of rainfall. This seasonality is reason to reevaluate the idea that Saharan rainfall is highly irregular and unpredictable.
C1 [Kelley, Owen A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Kelley, Owen A.] George Mason Univ, Ctr Earth Observing & Space Res, Fairfax, VA 22030 USA.
RP Kelley, OA (reprint author), NASA, Goddard Space Flight Ctr, Code 610-2, Greenbelt, MD 20771 USA.
EM owen.kelley@nasa.gov
FU NASA METS-II [NNG10CR16C]
FX This work was supported by the NASA METS-II Contract NNG10CR16C. The
Precipitation Processing System (PPS) at NASA Goddard Space Flight
Center provided computational facilities. The staff of the NASA Goddard
Library located hard-to-find documents and datasets. The following
people provided suggestions for improving the manuscript: Jeanne Beatty,
Michael Chesnes, George Huffman, Genevieve Demos Kelley, Erich Stocker,
John Stout, Clifton Sutton, and three anonymous reviewers.
NR 85
TC 3
Z9 3
U1 2
U2 9
PU AMER METEOROLOGICAL SOC
PI BOSTON
PA 45 BEACON ST, BOSTON, MA 02108-3693 USA
SN 0894-8755
EI 1520-0442
J9 J CLIMATE
JI J. Clim.
PD SEP
PY 2014
VL 27
IS 18
BP 6919
EP 6939
DI 10.1175/JCLI-D-14-00145.1
PG 21
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA AP3NC
UT WOS:000341981800005
ER
PT J
AU Blaber, EA
Dvorochkin, N
Torres, ML
Yousuf, R
Burns, BP
Globus, RK
Almeida, EAC
AF Blaber, E. A.
Dvorochkin, N.
Torres, M. L.
Yousuf, R.
Burns, B. P.
Globus, R. K.
Almeida, E. A. C.
TI Mechanical unloading of bone in microgravity reduces mesenchymal and
hematopoietic stem cell-mediated tissue regeneration
SO STEM CELL RESEARCH
LA English
DT Article
ID RED-BLOOD-CELL; EPIDERMAL-GROWTH-FACTOR; OSTEOCLAST DIFFERENTIATION;
SPACE-FLIGHT; OSTEOBLAST DIFFERENTIATION; SIMULATED MICROGRAVITY;
MUSCULOSKELETAL DISUSE; PRESSURE-GRADIENTS; CANCELLOUS BONE;
GENE-EXPRESSION
AB Mechanical loading of mammalian tissues is a potent promoter of tissue growth and regeneration, whilst unloading in microgravity can cause reduced tissue regeneration, possibly through effects on stem cell tissue progenitors. To test the specific hypothesis that mechanical unloading alters differentiation of bone marrow mesenchymal and hematopoietic stem cell lineages, we studied cellular and molecular aspects of how bone marrow in the mouse proximal femur responds to unloading in microgravity. Trabecular and cortical endosteal bone surfaces in the femoral head underwent significant bone resorption in microgravity, enlarging the marrow cavity. Cells isolated from the femoral head marrow compartment showed significant down-regulation of gene expression markers for early mesenchymal and hematopoietic differentiation, including FUT1(-6.72), CSF2(-3.30), CD90(-3.33), PTPRC(-2.79), and GDF15(-2.45), but not stem cell markers, such as SOX2. At the cellular level, in situ histological analysis revealed decreased megakaryocyte numbers whilst erythrocytes were increased 2.33 fold. Furthermore, erythrocytes displayed elevated fucosylation and clustering adjacent to sinuses forming the marrow-blood barrier, possibly providing a mechanistic basis for explaining spaceflight anemia. Culture of isolated bone marrow cells immediately after microgravity exposure increased the marrow progenitor's potential for mesenchymal differentiation into in-vitro mineralized bone nodules, and hematopoietic differentiation into osteoclasts, suggesting an accumulation of undifferentiated progenitors during exposure to microgravity. These results support the idea that mechanical unloading of mammalian tissues in microgravity is a strong inhibitor of tissue growth and regeneration mechanisms, acting at the level of early mesenchymal and hematopoietic stem cell differentiation. Published by Elsevier B. V.
C1 [Blaber, E. A.; Burns, B. P.] Univ New S Wales, Sch Biotechnol & Bimol Sci, Sydney, NSW, Australia.
[Blaber, E. A.; Dvorochkin, N.; Torres, M. L.; Yousuf, R.; Globus, R. K.; Almeida, E. A. C.] NASA, Ames Res Ctr, Space Biosci Div, Moffett Field, CA 94035 USA.
[Torres, M. L.] Santa Clara Univ, Dept Bioengn, Santa Clara, CA 95053 USA.
RP Almeida, EAC (reprint author), NASA, Ames Res Ctr, Mail Stop 236-7, Moffett Field, CA 94035 USA.
EM e.almeida@nasa.gov
OI BURNS, BRENDAN/0000-0002-2962-2597
NR 97
TC 10
Z9 10
U1 1
U2 11
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 1873-5061
EI 1876-7753
J9 STEM CELL RES
JI Stem Cell Res.
PD SEP
PY 2014
VL 13
IS 2
BP 181
EP 201
DI 10.1016/j.scr.2014.05.005
PG 21
WC Cell & Tissue Engineering; Biotechnology & Applied Microbiology; Cell
Biology
SC Cell Biology; Biotechnology & Applied Microbiology
GA AP7WB
UT WOS:000342287400001
PM 25011075
ER
PT J
AU Chen, BY
Pinho, ST
De Carvalho, NV
Baiz, PM
Tay, TE
AF Chen, B. Y.
Pinho, S. T.
De Carvalho, N. V.
Baiz, P. M.
Tay, T. E.
TI A floating node method for the modelling of discontinuities in
composites
SO ENGINEERING FRACTURE MECHANICS
LA English
DT Article
DE Composites; Phantom node method; X-FEM; Multiple cracks; Crack
interaction
ID FINITE-ELEMENT-METHOD; 3-DIMENSIONAL CRACK INITIATION; FIBER-REINFORCED
COMPOSITES; POSTERIORI ERROR ESTIMATION; DEFORMABLE SHALLOW SHELLS;
AUTOMATIC MESH GENERATOR; COHESIVE SEGMENTS METHOD; THIN-WALLED
STRUCTURES; ANALYSES SGBEM-FEM; LEVEL SETS
AB This paper presents a new method suitable for modelling multiple discontinuities within a finite element. The architecture of the proposed method is similar to that of the phantom node method (which is equivalent to XFEM with Heaviside enrichment), and the solution of it is equivalent to local remeshing within the cracked element. The new method shows several advantages over the phantom node method, such as avoiding errors in the mapping of the crack geometry from the physical to the natural space and avoiding performing integrations over only part of an element. Compared to remeshing, the proposed method enables the representation of discontinuities through relatively closed FE codes (such as user-defined elements) without modifying the initial mesh and geometry, thus making it computationally more efficient. Additionally, the proposed method is particularly suited for modelling weak and cohesive discontinuities and for the representation of complex crack networks; it can model multiple plies and interfaces of a composite laminate, and both matrix crack and delamination, within a user-defined element; the information is shared between the plies and interfaces within such an element, allowing the direct implementation of interactive mechanisms. Verification examples show that the floating node method can predict stress intensity factors and crack propagation accurately. An application example shows that the proposed method can predict well the transition from matrix cracking to delamination and the subsequent saturation of matrix crack density in a c ross-ply laminate. (C) 2014 Elsevier Ltd. All rights reserved.
C1 [Chen, B. Y.; Tay, T. E.] Natl Univ Singapore, Dept Mech Engn, Singapore 119077, Singapore.
[Chen, B. Y.; Pinho, S. T.; Baiz, P. M.] Univ London Imperial Coll Sci Technol & Med, Dept Aeronaut, London SW7 2AZ, England.
[De Carvalho, N. V.] NASA, Langley Res Ctr, Natl Inst Aerosp, Hampton, VA 23665 USA.
RP Chen, BY (reprint author), Block EA,02-21,9 Engn Dr 1, Singapore 117576, Singapore.
EM boyang.chen@nus.edu.sg
RI Pinho, Silvestre/B-4618-2012; Chen, Boyang/J-1271-2016;
OI Chen, Boyang/0000-0001-7393-4363; Tay, Tong-Earn/0000-0002-2846-1947
FU National University of Singapore
FX The first author greatly acknowledges the research scholarship from
National University of Singapore.
NR 134
TC 15
Z9 15
U1 2
U2 18
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0013-7944
EI 1873-7315
J9 ENG FRACT MECH
JI Eng. Fract. Mech.
PD SEP
PY 2014
VL 127
BP 104
EP 134
DI 10.1016/j.engfracmech.2014.05.018
PG 31
WC Mechanics
SC Mechanics
GA AO7SA
UT WOS:000341551700010
ER
PT J
AU Siljestrom, S
Freissinet, C
Goesmann, F
Steininger, H
Goetz, W
Steele, A
Amundsen, H
AF Siljestrom, Sandra
Freissinet, Caroline
Goesmann, Fred
Steininger, Harald
Goetz, Walter
Steele, Andrew
Amundsen, Hans
CA AMASE11 Team
TI Comparison of Prototype and Laboratory Experiments on MOMA GCMS: Results
from the AMASE11 Campaign
SO ASTROBIOLOGY
LA English
DT Article
DE MOMA; ExoMars; Pyrolysis-GCMS; Derivatization; Svalbard; AMASE
ID CHROMATOGRAPHY-MASS-SPECTROMETRY; ALLAN HILLS 84001; MARTIAN METEORITE
ALH84001; ROCKNEST AEOLIAN DEPOSIT; MARS-LIKE SOILS; ORGANIC-COMPOUNDS;
OMEGA/MARS EXPRESS; DESERT VARNISH; LIFE-DETECTION; FOSSIL LEAVES
AB The characterization of any organic molecules on Mars is a top-priority objective for the ExoMars European Space Agency-Russian Federal Space Agency joint mission. The main instrument for organic analysis on the ExoMars rover is the Mars Organic Molecule Analyzer (MOMA).
In preparation for the upcoming mission in 2018, different Mars analog samples are studied with MOMA and include samples collected during the Arctic Mars Analog Svalbard Expedition (AMASE) to Svalbard, Norway. In this paper, we present results obtained from two different Mars analog sites visited during AMASE11, Colletthogda and Botniahalvoya. Measurements were performed on the samples during AMASE11 with a MOMA gas chromatograph (GC) prototype connected to a commercial mass spectrometer (MS) and later in home institutions with commercial pyrolysis-GCMS instruments. In addition, derivatization experiments were performed on the samples during AMASE11 and in the laboratory. Three different samples were studied from the Colletthogda that included one evaporite and two carbonate-bearing samples. Only a single sample was studied from the Botniahalvoya site, a weathered basalt covered by a shiny surface consisting of manganese and iron oxides.
Organic molecules were detected in all four samples and included aromatics, long-chained hydrocarbons, amino acids, nucleobases, sugars, and carboxylic acids. Both pyrolysis and derivatization indicated the presence of extinct biota by the detection of carboxylic acids in the samples from Colletthogda, while the presence of amino acids, nucleobases, carboxylic acids, and sugars indicated an active biota in the sample from Botniahalvoya.
The results obtained with the prototype flight model in the field coupled with repeat measurements with commercial instruments within the laboratory were reassuringly similar. This demonstrates the performance of the MOMA instrument and validates that the instrument will aid researchers in their efforts to answer fundamental questions regarding the speciation and possible source of organic content on Mars.
C1 [Siljestrom, Sandra] SP Tech Res Inst Sweden, Dept Chem Mat & Surfaces, S-50115 Boras, Sweden.
[Siljestrom, Sandra; Steele, Andrew] Carnegie Inst Sci, Geophys Lab, Washington, DC USA.
[Freissinet, Caroline] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Freissinet, Caroline] Oak Ridge Associated Univ, NASA Postdoctoral Program NPP, Oak Ridge, TN USA.
[Goesmann, Fred; Steininger, Harald; Goetz, Walter] Max Planck Inst Sonnensyst Forsch, Gottingen, Germany.
[Amundsen, Hans] Earth & Planetary Explorat Serv, Oslo, Norway.
RP Siljestrom, S (reprint author), SP Tech Res Inst Sweden, Dept Chem Mat & Surfaces, Box 587, S-50115 Boras, Sweden.
EM sandra.siljestrom@sp.se
FU AMASE by ESA; Deutsches Zentrum fur Luft- und Raumfahrt (DLR) [FKZ:
50QX1001]; MPS; Swedish National Space Board; Deep Carbon Observatory
(A. Steele, PI); program of the Geophysical Laboratory, Carnegie
Institution of Washington; Swedish National Space Board [121/11]; GSFC;
NASA ASTEP (A. Steele, PI)
FX The financial support of AMASE by ESA is gratefully acknowledged. The
participation of F. G. was supported by Deutsches Zentrum fur Luft- und
Raumfahrt (DLR; FKZ: 50QX1001). The participation of S. S. in AMASE11
was supported by MPS and a Swedish National Space Board travel grant. S.
S. was further supported by the Deep Carbon Observatory (A. Steele, PI),
the postdoctoral fellowship program of the Geophysical Laboratory,
Carnegie Institution of Washington, and the Swedish National Space Board
(Contract No. 121/11). The participation of C. F. was supported by GSFC.
AMASE11 was strongly supported by NASA ASTEP (A. Steele, PI).
NR 89
TC 2
Z9 2
U1 5
U2 30
PU MARY ANN LIEBERT, INC
PI NEW ROCHELLE
PA 140 HUGUENOT STREET, 3RD FL, NEW ROCHELLE, NY 10801 USA
SN 1531-1074
EI 1557-8070
J9 ASTROBIOLOGY
JI Astrobiology
PD SEP
PY 2014
VL 14
IS 9
BP 780
EP 797
DI 10.1089/ast.2014.1197
PG 18
WC Astronomy & Astrophysics; Biology; Geosciences, Multidisciplinary
SC Astronomy & Astrophysics; Life Sciences & Biomedicine - Other Topics;
Geology
GA AP1GM
UT WOS:000341815900004
PM 25238325
ER
PT J
AU Heller, R
Williams, D
Kipping, D
Limbach, MA
Turner, E
Greenberg, R
Sasaki, T
Bolmont, E
Grasset, O
Lewis, K
Barnes, R
Zuluaga, JI
AF Heller, Rene
Williams, Darren
Kipping, David
Limbach, Mary Anne
Turner, Edwin
Greenberg, Richard
Sasaki, Takanori
Bolmont, Emeline
Grasset, Olivier
Lewis, Karen
Barnes, Rory
Zuluaga, Jorge I.
TI Formation, Habitability, and Detection of Extrasolar Moons
SO ASTROBIOLOGY
LA English
DT Review
DE Astrobiology; Extrasolar planets; Habitability; Planetary science; Tides
ID TRANSIT TIMING VARIATIONS; TIME-SERIES PHOTOMETRY; SOLAR-LIKE STARS;
GIANT PLANETS; GALILEAN SATELLITES; LIGHT CURVES; SOUTH-POLE; REGULAR
SATELLITES; TIDAL DISSIPATION; SUBSURFACE OCEAN
AB The diversity and quantity of moons in the Solar System suggest a manifold population of natural satellites exist around extrasolar planets. Of peculiar interest from an astrobiological perspective, the number of sizable moons in the stellar habitable zones may outnumber planets in these circumstellar regions. With technological and theoretical methods now allowing for the detection of sub-Earth-sized extrasolar planets, the first detection of an extrasolar moon appears feasible. In this review, we summarize formation channels of massive exomoons that are potentially detectable with current or near-future instruments. We discuss the orbital effects that govern exomoon evolution, we present a framework to characterize an exomoon's stellar plus planetary illumination as well as its tidal heating, and we address the techniques that have been proposed to search for exomoons. Most notably, we show that natural satellites in the range of 0.1-0.5 Earth mass (i) are potentially habitable, (ii) can form within the circumplanetary debris and gas disk or via capture from a binary, and (iii) are detectable with current technology.
C1 [Heller, Rene] McMaster Univ, Dept Phys & Astron, Origins Inst, Hamilton, ON L8S 4M1, Canada.
[Williams, Darren] Penn State Erie, Behrend Coll, Sch Sci, Erie, PA USA.
[Kipping, David] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Limbach, Mary Anne; Turner, Edwin] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA.
[Limbach, Mary Anne] Princeton Univ, Dept Mech & Aerosp Engn, Princeton, NJ 08544 USA.
[Turner, Edwin] Univ Tokyo, Kavli Inst Phys & Math Universe, Kashiwa, Chiba, Japan.
[Greenberg, Richard] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA.
[Sasaki, Takanori] Kyoto Univ, Dept Astron, Kyoto, Japan.
[Bolmont, Emeline] Univ Bordeaux, LAB, UMR 5804, Floirac, France.
[Bolmont, Emeline] CNRS, LAB, UMR 5804, Floirac, France.
[Grasset, Olivier] Univ Nantes, CNRS, Nantes, France.
[Lewis, Karen] Tokyo Inst Technol, Tokyo 152, Japan.
[Barnes, Rory] Univ Washington, Dept Astron, Seattle, WA 98195 USA.
[Barnes, Rory] NASA, Astrobiol Inst, Virtual Planetary Lab, Lead Team, Washington, DC USA.
[Zuluaga, Jorge I.] Univ Antioquia, FACom, FCEN, Inst Fis, Medellin, Colombia.
RP Heller, R (reprint author), McMaster Univ, Dept Phys & Astron, Origins Inst, Hamilton, ON L8S 4M1, Canada.
EM rheller@physics.mcmaster.ca
OI Zuluaga, Jorge I./0000-0002-6140-3116
FU Origins Institute at McMaster University; Canadian Astrobiology Training
Program, a Collaborative Research and Training Experience Program -
Natural Sciences and Engineering Research Council of Canada (NSERC);
Pennsylvania State University; Eberly College of Science; Pennsylvania
Space Grant Consortium; Global COE Program, "From the Earth to
'Earths,''' MEXT, Japan; JSPS KAKENHI [24740120]; NSF [AST-1108882];
NASA Astrobiology Institute [NNH05ZDA001C]; CODI/UdeA; World Premier
International Research Center Initiative, MEXT, Japan
FX The helpful comments of two referees are very much appreciated. We thank
Alexis Carlotti, Jill Knapp, Matt Mountain, George Rieke, Dave Spiegel,
and Scott Tremaine for useful conversations and Ted Stryk for granting
permission to use a reprocessed image of Europa. Rene Heller is
supported by the Origins Institute at McMaster University and by the
Canadian Astrobiology Training Program, a Collaborative Research and
Training Experience Program funded by the Natural Sciences and
Engineering Research Council of Canada (NSERC). Darren Williams is a
member of the Center for Exoplanets and Habitable Worlds, which is
supported by the Pennsylvania State University, the Eberly College of
Science, and the Pennsylvania Space Grant Consortium. Takanori Sasaki
was supported by a grant for the Global COE Program, "From the Earth to
'Earths,''' MEXT, Japan, and Grant-in-Aid for Young Scientists (B), JSPS
KAKENHI Grant Number 24740120. Rory Barnes acknowledges support from NSF
grant AST-1108882 and the NASA Astrobiology Institute's Virtual
Planetary Laboratory lead team under cooperative agreement no.
NNH05ZDA001C. Jorge I. Zuluaga is supported by CODI/UdeA. This research
has been supported in part by World Premier International Research
Center Initiative, MEXT, Japan. This work has made use of NASA's
Astrophysics Data System Bibliographic Services.
NR 261
TC 20
Z9 20
U1 4
U2 24
PU MARY ANN LIEBERT, INC
PI NEW ROCHELLE
PA 140 HUGUENOT STREET, 3RD FL, NEW ROCHELLE, NY 10801 USA
SN 1531-1074
EI 1557-8070
J9 ASTROBIOLOGY
JI Astrobiology
PD SEP
PY 2014
VL 14
IS 9
BP 798
EP 835
DI 10.1089/ast.2014.1147
PG 38
WC Astronomy & Astrophysics; Biology; Geosciences, Multidisciplinary
SC Astronomy & Astrophysics; Life Sciences & Biomedicine - Other Topics;
Geology
GA AP1GM
UT WOS:000341815900005
PM 25147963
ER
PT J
AU Ballard, T
Seager, R
Smerdon, JE
Cook, BI
Ray, AJ
Rajagopalan, B
Kushnir, Y
Nakamura, J
Henderson, N
AF Ballard, Tristan
Seager, Richard
Smerdon, Jason E.
Cook, Benjamin I.
Ray, Andrea J.
Rajagopalan, Balaji
Kushnir, Yochanan
Nakamura, Jennifer
Henderson, Naomi
TI Hydroclimate Variability and Change in the Prairie Pothole Region, the
"Duck Factory'' of North America
SO EARTH INTERACTIONS
LA English
DT Article
DE North America; Climate change; Hydrologic cycle; Climate variability;
Ecosystem effects
ID WETLANDS; CLIMATE; VULNERABILITY; SURVIVAL; DROUGHT; DAKOTA; ENSO
AB The Prairie Pothole Region (PPR) of the northern Great Plains is a vital ecosystem responsible each year for producing 50%-80% of new recruits to the North American duck population. Climate variability and change can impact the hydrology and ecology of the region with implications for waterfowl populations. The historical relationship between PPR wetlands, duck populations, and seasonal hydroclimate are explored. Model experiments from phase 5 of the Coupled Model Intercomparison Project are used to determine whether a recent wetting trend is due to natural variability or changing climate and how PPR hydroclimate will change into the future. Year-to-year variations in May duck populations, pond numbers, and the Palmer drought severity index are well correlated over past decades. Pond and duck numbers tend to increase in spring following La Nina events, but the correlation is not strong. Model simulations suggest that the strengthening of the precipitation gradient across the PPR over the past century is predominantly due to natural variability and therefore could reverse. Model projections of future climate indicate precipitation will increase across the PPR in all seasons except summer, but this gain for surface moisture is largely offset by increased evapotranspiration because of higher temperatures and increased atmospheric evaporative demand. In summer, the combined effects of warming and precipitation changes indicate seasonal surface drying in the future. The presented hydroclimate analyses produce potential inputs to ecological and hydrological simulations of PPR wetlands to inform risk analysis of how this North American waterfowl habitat will evolve in the future, providing guidance to land managers facing conservation decisions.
C1 [Ballard, Tristan] Duke Univ, Durham, NC USA.
[Seager, Richard; Smerdon, Jason E.; Kushnir, Yochanan; Nakamura, Jennifer; Henderson, Naomi] Columbia Univ, Lamont Doherty Earth Observ, Palisades, NY 10964 USA.
[Cook, Benjamin I.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
[Ray, Andrea J.] NOAA, Earth Syst Res Lab, Boulder, CO USA.
[Rajagopalan, Balaji] Univ Colorado, Dept Civil Environm & Architectural Engn, Boulder, CO 80309 USA.
RP Seager, R (reprint author), Columbia Univ, Lamont Doherty Earth Observ, 61 Route 9W, Palisades, NY 10964 USA.
EM seager@ldeo.columbia.edu
RI Smerdon, Jason/F-9952-2011; Cook, Benjamin/H-2265-2012; Rajagopalan,
Balaji/A-5383-2013
OI Rajagopalan, Balaji/0000-0002-6883-7240
FU NSF [AGS-1243204]; NOAA [NA08OAR4320912]; Lamont summer undergraduate
intern program
FX This work was supported by NSF Award AGS-1243204 ("Linking near-term
future changes in weather and hydroclimate in western North America to
adaptation for ecosystem and water management") and NOAA Award
NA08OAR4320912 ("Global decadal hydroclimate variability and change").
We particularly thank Susan Skagen (U.S. Geological Survey), Michael
Olson and Richard Nelson (U.S. Fish and Wildlife Service), and Helen
Sofaer (Colorado State University) for their careful readings, which led
to a more informative and practically useful paper. TB acknowledges the
Lamont summer undergraduate intern program for additional support. We
thank Haibo Liu for assembling the CMIP5 model database at Lamont. We
thank two anonymous reviewers for detailed and thoughtful comments and
criticisms. The authors declare no conflicts of interest.
NR 36
TC 6
Z9 6
U1 4
U2 43
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 1087-3562
J9 EARTH INTERACT
JI Earth Interact.
PD SEP
PY 2014
VL 18
AR 14
DI 10.1175/EI-D-14-0004.1
PG 28
WC Geosciences, Multidisciplinary
SC Geology
GA AP1GI
UT WOS:000341815500001
ER
PT J
AU Yau, AJ
Lenihan, HS
Kendall, BE
AF Yau, Annie J.
Lenihan, Hunter S.
Kendall, Bruce E.
TI Fishery management priorities vary with self-recruitment in sedentary
marine populations
SO ECOLOGICAL APPLICATIONS
LA English
DT Article
DE closed population; coral reef fishery; fishing mortality; giant clam;
integral projection model; local population; mixed recruitment; Mo'orea,
French Polynesia; open population; self-recruitment; small-scale
fishery; Tridacna
ID CORAL-REEF FISHERIES; GIANT CLAMS; LARVAL CONNECTIVITY;
DENSITY-DEPENDENCE; TRIDACNA-CROCEA; MAXIMA; MODEL; GROWTH;
SUSTAINABILITY; ARCHIPELAGO
AB Fisheries science often uses population models that assume no external recruitment, but nearshore marine populations harvested on small scales of <200 km often exhibit an unknown mix of self-recruitment and recruitment from external sources. Since empirical determination of self-recruitment vs. external recruitment is difficult, we used a modeling approach to examine the sensitivity of fishery management priorities to recruitment assumptions (self [closed], external [open]) in a local population of harvested giant clams (Tridacna maxima) on Mo'orea, French Polynesia. From 2006 to 2010, we measured growth, fecundity, recruitment, and survival (resulting from natural and fishing mortality). We used these data to parameterize both a closed (complete self-recruitment) and an open (no self-recruitment) integral projection model (IPM), and then calculated elasticities of demographic rates (growth, survival, recruitment) to future population abundance in 20 years. The models' lowest projected abundance was 93.4% (95% CI, [86.5%, 101.8%]) of present abundance, if the local population is entirely open and the present level of fishing mortality persists. The population will exhibit self-sustaining dynamics (1 <= lambda <= 1.07) as for a closed population if the ratio of self-recruits per gram of dry gonad is >0.775 (equivalent to 52.85% self-recruitment under present conditions). Elasticity analysis of demographic parameters indicated that future abundance can most effectively be influenced by increasing survival of mid-sized clams (similar to 80-120 mm) if the population is self-sustaining, and by increasing survival of juvenile clams (similar to 40-70 mm) if the population is non-self-sustaining (as for an open population). Our results illustrate that management priorities can vary depending on the amount of self-recruitment in a local population.
C1 [Yau, Annie J.; Lenihan, Hunter S.; Kendall, Bruce E.] Univ Calif Santa Barbara, Bren Sch Environm Sci & Management, Santa Barbara, CA 93106 USA.
RP Yau, AJ (reprint author), NOAA, Pacific Isl Fisheries Sci Ctr, Natl Marine Fisheries Serv, 1845 Wasp Blvd,Bldg 176, Honolulu, HI 96818 USA.
EM annie.yau@noaa.gov
RI Kendall, Bruce/C-1871-2008
OI Kendall, Bruce/0000-0003-1782-8106
FU Gump Research Station Pacific Education and Research Laboratories
(PEARL) Award; PADI Foundation [317]; Luce Science to Solutions
Fellowship; Mo'orea Coral Reef (MCR) Long Term Ecological Research Site;
Bren School of Environmental Science and Management; University of
California
FX This research was supported by grants to A. Yau from the Gump Research
Station Pacific Education and Research Laboratories (PEARL) Award, PADI
Foundation grant number 317, and the Luce Science to Solutions
Fellowship. Additional support came from the Mo'orea Coral Reef (MCR)
Long Term Ecological Research Site, the Bren School of Environmental
Science and Management, and the University of California. This is a
contribution of the MCR LTER Site and Contribution Number 195 of the UC
Berkeley Gump Research Station. We thank R. Nisbet and J. Wilson for
their input and helpful comments that improved earlier versions of the
manuscript. We thank the staff of the Gump Station for their assistance
and friendship. We are grateful to T. Adam, A. Brooks, X. Han, K.
Seydel, H. Stewart, and K. Walovich for their efforts in collecting
shells. Finally, we thank L. Albertson, J. Creason, T. Minter, A.
Rivera, S. Shaffiy, and T. Teore for their assistance with fieldwork,
all the fishers for their knowledge on pahua fishing and participation
in this study, and the Brando Trust, Conservation Tetiaroa, and Pacific
Beachcomber for permission to work on Tetiaroa.
NR 63
TC 3
Z9 3
U1 1
U2 31
PU ECOLOGICAL SOC AMER
PI WASHINGTON
PA 1990 M STREET NW, STE 700, WASHINGTON, DC 20036 USA
SN 1051-0761
EI 1939-5582
J9 ECOL APPL
JI Ecol. Appl.
PD SEP
PY 2014
VL 24
IS 6
BP 1490
EP 1504
PG 15
WC Ecology; Environmental Sciences
SC Environmental Sciences & Ecology
GA AO9YE
UT WOS:000341715800018
ER
PT J
AU Sujidkul, T
Smith, CE
Ma, ZJ
Morscher, GN
Xia, ZH
AF Sujidkul, Thanyawalai
Smith, Craig E.
Ma, Zhijun
Morscher, Gregory N.
Xia, Zhenhai
TI Correlating Electrical Resistance Change with Mechanical Damage in Woven
SiC/SiC Composites: Experiment and Modeling
SO JOURNAL OF THE AMERICAN CERAMIC SOCIETY
LA English
DT Article
ID DEPENDENT MATRIX CRACKING; CERAMIC COMPOSITES; CFRP COMPOSITES;
ACCUMULATION; RESISTIVITY; BEHAVIOR; FAILURE
AB Silicon carbide (SiC) fiber-reinforced SiC matrix composites are inherently multifunctional materials. In addition to their primary function as a structural material, the electric properties of the SiC/SiC composites could be used for the sensing and monitoring of in situ damage nucleation and evolution. To detect damage and use that information to further predict the useful life of a particular component, it is necessary to establish the relationship between damage and electrical resistance change. Here, two typical SiC/SiC composites, melt infiltrated (MI), and chemical vapor infiltrated (CVI) woven SiC/SiC composites, were tested to establish the relationship between the electrical response and mechanical damage in unload-reload tensile hysteresis tests. Compared to the 55% resistance increase seen for CVI composites, the MI SiC/SiC composites exhibit a maximum resistance change in 450% in response to mechanical loading (damage), which is the highest sensitivity known among various composites. An analytic model accounting for fiber breakage and matrix cracks was developed to link the electrical resistance to mechanical damage in the composites. The predictions from the models agree well with the experimental data for both composites with high and low conductive matrices. The residual resistance change after unloading is also correlated to the loading history by the analytical relationship. This study demonstrates that resistance change is sensitive to damage in a predictable manner and can be used to improve the reliability of damage assessment of SiC/SiC composites.
C1 [Sujidkul, Thanyawalai; Morscher, Gregory N.] Univ Akron, Dept Mech Engn, Akron, OH 44325 USA.
[Smith, Craig E.] NASA, Glenn Res Ctr, Ohio Aerosp Inst, Ceram Branch, Cleveland, OH 44135 USA.
[Ma, Zhijun] Xian Univ Technol, Sch Mat Sci & Engn, Xian, Peoples R China.
[Xia, Zhenhai] Univ N Texas, Dept Chem, Dept Mat Sci & Engn, Denton, TX 76203 USA.
RP Xia, ZH (reprint author), Univ N Texas, Dept Chem, Dept Mat Sci & Engn, Denton, TX 76203 USA.
EM zhenhai.xia@unt.edu
FU NASA Glenn Research Center ARMD Hypersonics program [NNX07AN56H]; NSF
[CMMI-1212259, CMMI-1266295]
FX We would like to thank the NASA Glenn Research Center ARMD Hypersonics
program for the support of the graduate student research program under
contract NNX07AN56H and the Glenn Research Center Ceramics branch for
use of their research facilities. The project is also supported
partially by NSF (CMMI-1212259 and CMMI-1266295).
NR 26
TC 1
Z9 1
U1 2
U2 17
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 0002-7820
EI 1551-2916
J9 J AM CERAM SOC
JI J. Am. Ceram. Soc.
PD SEP
PY 2014
VL 97
IS 9
BP 2936
EP 2942
DI 10.1111/jace.13019
PG 7
WC Materials Science, Ceramics
SC Materials Science
GA AP1JX
UT WOS:000341826500037
ER
PT J
AU Chen, YC
Christensen, MW
Stephens, GL
Seinfeld, JH
AF Chen, Yi-Chun
Christensen, Matthew W.
Stephens, Graeme L.
Seinfeld, John H.
TI Satellite-based estimate of global aerosol-cloud radiative forcing by
marine warm clouds
SO NATURE GEOSCIENCE
LA English
DT Article
ID GENERAL-CIRCULATION MODEL; OPTICAL DEPTH; STRATOCUMULUS; ALBEDO;
REANALYSIS; ALGORITHM; COVER
AB Changes in aerosol concentrations affect cloud albedo and Earth's radiative balance(1). Aerosol radiative forcing from pre-industrial time to the present due to the effect of atmospheric aerosol levels on the micro- and macrophysics of clouds bears the largest uncertainty among external influences on climate change(1). Of all cloud forms, low-level marine clouds exert the largest impact on the planet's albedo(2). For example, a 6% increase in the albedo of global marine stratiform clouds could offset the warming that would result from a doubling of atmospheric CO2 concentrations(3). Marine warm cloud properties are thought to depend on aerosol levels and large-scale dynamic or thermodynamic states(4-6). Here we present a comprehensive analysis of multiple measurements from the A-Train constellation of Earth-observing satellites, to quantify the radiative forcing exerted by aerosols interacting with marine clouds. Specifically, we analyse observations of co-located aerosols and clouds over the world's oceans for the period August 2006-April 2011, comprising over 7.3 million CloudSat single-layer marine warm cloud pixels. We find that thermodynamic conditions-that is, tropospheric stability and humidity in the free troposphere-and the state of precipitation act together to govern the cloud liquid water responses to the presence of aerosols and the strength of aerosol-cloud radiative forcing.
C1 [Chen, Yi-Chun; Seinfeld, John H.] CALTECH, Pasadena, CA 91125 USA.
[Chen, Yi-Chun; Stephens, Graeme L.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Christensen, Matthew W.] Colorado State Univ, Ft Collins, CO 80523 USA.
RP Seinfeld, JH (reprint author), CALTECH, Pasadena, CA 91125 USA.
EM seinfeld@caltech.edu
RI Christensen, Matthew/C-5733-2013
FU Office of Naval Research grant [N00014-14-1-0097]
FX This work was supported by Office of Naval Research grant
N00014-14-1-0097.
NR 29
TC 22
Z9 23
U1 6
U2 29
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 SEP
PY 2014
VL 7
IS 9
BP 643
EP 646
DI 10.1038/NGEO2214
PG 4
WC Geosciences, Multidisciplinary
SC Geology
GA AO8WI
UT WOS:000341635600011
ER
PT J
AU Burton, AS
Grunsfeld, S
Elsila, JE
Glavin, DP
Dworkin, JP
AF Burton, Aaron S.
Grunsfeld, Sarah
Elsila, Jamie E.
Glavin, Daniel P.
Dworkin, Jason P.
TI The effects of parent-body hydrothermal heating on amino acid abundances
in CI-like chondrites
SO POLAR SCIENCE
LA English
DT Article
DE Meteorite; Amino acid; CI chondrite; Aqueous alteration; Thermal
metamorphism
ID CARBONACEOUS CHONDRITES; THERMAL METAMORPHISM; AQUEOUS ALTERATION; MASS
SPECTROMETRY; METEORITES; STABILITY; MURCHISON; CM; DECARBOXYLATION;
TEMPERATURES
AB We determined the amino acid abundances and enantiomeric compositions of the Antarctic CI1 carbonaceous chondrites Yamato (Y)-86029 and Y-980115, as well as the Ivuna and Orgueil CI1 carbonaceous chondrites by liquid chromatography with fluorescence detection and time-of-flight mass spectrometry. Y-86029 and Y-980115 both show evidence of parent-body heating (500-600 degrees C) in addition to aqueous alteration, while Ivuna and Orgueil only show evidence for aqueous alteration. In contrast to Ivuna and Orgueil, which each contain similar to 70 nmol/g of amino acids in acid-hydrolyzed, water extracts, both heated Yamato CI meteorites contain only low levels of amino acids that were primarily L-enantiomers of proteinogenic amino acids, indicating that they are likely to be terrestrial in origin. Because indigenous amino acids have been found in meteorites that have experienced metamorphic temperatures of >1000 degrees C with only minimal aqueous alteration, heating alone is not sufficient to explain the lack of amino acids in Y-86029 and Y-980115. Rather, our data suggest that the combination of heating and aqueous alteration has a profound destructive effect on amino acids in meteorites. This finding has implications for the origins of amino acids and other molecules in the early evolution of our solar system. Published by Elsevier B.V. and NIPR.
C1 [Burton, Aaron S.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA.
[Burton, Aaron S.; Grunsfeld, Sarah; Elsila, Jamie E.; Glavin, Daniel P.; Dworkin, Jason P.] NASA, Goddard Space Flight Ctr, Solar Syst Explorat Div, Greenbelt, MD 20771 USA.
[Grunsfeld, Sarah] River Hill High Sch, Clarksville, MD 21029 USA.
RP Burton, AS (reprint author), NASA, Lyndon B Johnson Space Ctr, KR,2101 NASA Pkwy, Houston, TX 77058 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 Cosmochemistry Program;
Simons Foundation (SCOL) [302497]; NASA Postdoctoral Program at the
Goddard Space Flight Center; NASA; Gifted and Talented Education Program
of the Howard County Public School System
FX We thank the National Institute of Polar Research of Japan for the
Yamato meteorite samples, the Natural History Museum of the United
Kingdom for the Ivuna sample, and the Musee National of Paris for the
sample of Orgueil. J.E.E., D.P.G. and J.P.D. acknowledge funding support
from the National Aeronautics and Space Administration (NASA)
Astrobiology Institute, the Goddard Center for Astrobiology and the NASA
Cosmochemistry Program. This work was also supported in part by a grant
from the Simons Foundation (SCOL award 302497 to J.P.D.). A.S.B.
acknowledges support from the NASA Postdoctoral Program at the Goddard
Space Flight Center, administered by Oak Ridge Associated Universities
through a contract with NASA. S.G. acknowledges institutional support
through the Gifted and Talented Education Program of the Howard County
Public School System.
NR 47
TC 10
Z9 10
U1 1
U2 18
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 1873-9652
EI 1876-4428
J9 POLAR SCI
JI Polar Sci.
PD SEP
PY 2014
VL 8
IS 3
BP 255
EP 263
DI 10.1016/j.polar.2014.05.002
PG 9
WC Ecology; Geosciences, Multidisciplinary
SC Environmental Sciences & Ecology; Geology
GA AP0YW
UT WOS:000341793800005
ER
PT J
AU Numata, K
Wu, S
Riris, H
AF Numata, Kenji
Wu, Stewart
Riris, Haris
TI Fast-switching methane lidar transmitter based on a seeded optical
parametric oscillator
SO APPLIED PHYSICS B-LASERS AND OPTICS
LA English
DT Article
ID DIFFERENTIAL ABSORPTION LIDAR; ATMOSPHERIC CARBON-DIOXIDE; CO2 COLUMN
ABSORPTION; FREQUENCY STABILIZATION; AIRBORNE MEASUREMENTS; LASER;
SENSITIVITY; PHASE; SPECTROSCOPY; MODULATION
AB We report on our development effort for a trace-gas-sensing lidar transmitter to be used in future Earth-orbiting satellites. Our lidar transmitter is based on an optical parametric oscillator (OPO), whose output wavelength is switched at a rate of 5 kHz across the target line. The OPO cavity length and the seed laser wavelengths are stabilized to molecular and atomic references. We demonstrated the concept of the OPO-based lidar transmitter at 1,651 nm, achieving similar to 300-mu J output energy and < 300-MHz linewidth, which are anticipated to be required for a future methane lidar spaceborne mission.
C1 [Numata, Kenji] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Numata, Kenji; Wu, Stewart; Riris, Haris] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Numata, K (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
EM kenji.numata@nasa.gov
FU NASA Advanced Component Technology program
FX This research was funded by the NASA Advanced Component Technology
program. We would like to thank Dr. Stephan Kawa, Dr. Mark Stephen, Dr.
Steven Li, Dr. Jeffrey Chen, Dr. Jim Abshire, and Dr. Michael Krainak
for their support throughout the program. We would also like to thank
the Earth Science Technology Office (ESTO), the Instrument Incubator
Program, and the Goddard Space Flight Center IRAD program.
NR 29
TC 7
Z9 7
U1 0
U2 14
PU SPRINGER
PI NEW YORK
PA 233 SPRING ST, NEW YORK, NY 10013 USA
SN 0946-2171
EI 1432-0649
J9 APPL PHYS B-LASERS O
JI Appl. Phys. B-Lasers Opt.
PD SEP
PY 2014
VL 116
IS 4
BP 959
EP 966
DI 10.1007/s00340-014-5783-4
PG 8
WC Optics; Physics, Applied
SC Optics; Physics
GA AO5FQ
UT WOS:000341369600022
ER
PT J
AU Cordiner, MA
Remijan, AJ
Boissier, J
Milam, SN
Mumma, MJ
Charnley, SB
Paganini, L
Villanueva, G
Bockelee-Morvan, D
Kuan, YJ
Chuang, YL
Lis, DC
Biver, N
Crovisier, J
Minniti, D
Coulson, IM
AF Cordiner, M. A.
Remijan, A. J.
Boissier, J.
Milam, S. N.
Mumma, M. J.
Charnley, S. B.
Paganini, L.
Villanueva, G.
Bockelee-Morvan, D.
Kuan, Y-J.
Chuang, Y-L.
Lis, D. C.
Biver, N.
Crovisier, J.
Minniti, D.
Coulson, I. M.
TI MAPPING THE RELEASE OF VOLATILES IN THE INNER COMAE OF COMETS C/2012 F6
(LEMMON) AND C/2012 S1 (ISON) USING THE ATACAMA LARGE
MILLIMETER/SUBMILLIMETER ARRAY
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE comets: individual (C/2012 S1 (ISON), C/2012 F6 (Lemmon)); techniques:
interferometric
ID O1 HALE-BOPP; C/1995 O1; MOLECULAR OBSERVATIONS; INFRARED WAVELENGTHS;
ORGANIC-MOLECULES; EXTENDED SOURCES; FORMALDEHYDE; ORIGIN;
POLYOXYMETHYLENE; DEGRADATION
AB Results are presented from the first cometary observations using the Atacama Large Millimeter/Submillimeter Array (ALMA), including measurements of the spatially resolved distributions of HCN, HNC, H2CO, and dust within the comae of two comets: C/2012 F6 (Lemmon) and C/2012 S1 (ISON), observed at heliocentric distances of 1.5 AU and 0.54 AU, respectively. These observations (with angular resolution approximate to 0 ''.5), reveal an unprecedented level of detail in the distributions of these fundamental cometary molecules, and demonstrate the power of ALMA for quantitative measurements of the distributions of molecules and dust in the inner comae of typical bright comets. In both comets, HCN is found to originate from (or within a few hundred kilometers of) the nucleus, with a spatial distribution largely consistent with spherically symmetric, uniform outflow. By contrast, the HNC distributions are clumpy and asymmetrical, with peaks at cometocentric radii similar to 500-1000 km, consistent with release of HNC in collimated outflow(s). Compared to HCN, the H2CO distribution in comet Lemmon is very extended. The interferometric visibility amplitudes are consistent with coma production of H2CO and HNC from unidentified precursor material(s) in both comets. Adopting a Haser model, the H2CO parent scale length is found to be a few thousand kilometers in Lemmon and only a few hundred kilometers in ISON, consistent with the destruction of the precursor by photolysis or thermal degradation at a rate that scales in proportion to the solar radiation flux.
C1 [Cordiner, M. A.; Milam, S. N.; Mumma, M. J.; Charnley, S. B.; Paganini, L.; Villanueva, G.] NASA, Goddard Space Flight Ctr, Goddard Ctr Astrobiol, Greenbelt, MD 20771 USA.
[Cordiner, M. A.; Paganini, L.; Villanueva, G.] Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA.
[Remijan, A. J.] Natl Radio Astron Observ, Charlottesville, VA 22903 USA.
[Boissier, J.] IRAM, F-38406 St Martin Dheres, France.
[Bockelee-Morvan, D.; Biver, N.; Crovisier, J.] Univ Paris Diderot, CNRS, LEISA, Observ Paris,UPMC, F-92195 Meudon, France.
[Kuan, Y-J.; Chuang, Y-L.] Natl Taiwan Normal Univ, Taipei 116, Taiwan.
[Kuan, Y-J.] Acad Sinica, Inst Astron & Astrophys, Taipei 106, Taiwan.
[Lis, D. C.] Univ Paris 06, Sorbonne Univ, CNRS, Observ Paris,UMR 8112,LERMA, F-75014 Paris, France.
[Lis, D. C.] CALTECH, Cahill Ctr Astron & Astrophys 301 17, Pasadena, CA 91125 USA.
[Minniti, D.] Pontificia Univ Catolica Chile, Santiago, Chile.
[Minniti, D.] Univ Andres Bello, Dept Ciencias Fis, Santiago, Chile.
[Coulson, I. M.] Joint Astron Ctr, Hilo, HI 96720 USA.
RP Cordiner, MA (reprint author), NASA, Goddard Space Flight Ctr, Goddard Ctr Astrobiol, 8800 Greenbelt Rd, Greenbelt, MD 20771 USA.
EM martin.cordiner@nasa.gov
RI Milam, Stefanie/D-1092-2012
OI Milam, Stefanie/0000-0001-7694-4129
FU NASA Astrobiology Institute through the Goddard Center for Astrobiology;
NASA's Planetary Atmospheres and Planetary Astronomy Programs; NASA
through JPL/Caltech; Basal CATA [PFB-06]; ICM MAS; NSC
[99-2112-M-003-003-MY3, 100-2119-M-003-001-MY3]
FX This work was supported by the NASA Astrobiology Institute through the
Goddard Center for Astrobiology, and NASA's Planetary Atmospheres and
Planetary Astronomy Programs. It makes use of the following ALMA data:
ADS/JAO. ALMA #2012.A.00020.S and #2012.A.00033.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. The National Radio Astronomy Observatory is a
facility of the National Science Foundation operated under cooperative
agreement by Associated Universities, Inc. D. C. L. is supported by NASA
through JPL/Caltech. D. M. is supported by Basal CATA PFB-06 and the ICM
MAS. Y.J.K. is supported by NSC grants 99-2112-M-003-003-MY3 and
100-2119-M-003-001-MY3.
NR 30
TC 19
Z9 19
U1 1
U2 13
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 SEP 1
PY 2014
VL 792
IS 1
AR L2
DI 10.1088/2041-8205/792/1/L2
PG 6
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AO4KO
UT WOS:000341306900002
ER
PT J
AU Coutens, A
Jorgensen, JK
Persson, MV
van Dishoeck, EF
Vastel, C
Taquet, V
AF Coutens, A.
Jorgensen, J. K.
Persson, M. V.
van Dishoeck, E. F.
Vastel, C.
Taquet, V.
TI HIGH D2O/HDO RATIO IN THE INNER REGIONS OF THE LOW-MASS PROTOSTAR NGC
1333 IRAS2A
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE astrochemistry; ISM: individual objects (NGC 1333 IRAS2A); ISM:
molecules; stars: protostars
ID WATER DEUTERIUM FRACTIONATION; SOLAR-TYPE PROTOSTARS; DEUTERATED WATER;
HEAVY-WATER; INTERSTELLAR-MEDIUM; CHEMICAL HISTORY; STAR-FORMATION; WARM
WATER; MOLECULES; DISKS
AB Water plays a crucial role both in the interstellar medium and on Earth. To constrain its formation mechanisms and its evolution through the star formation process, the determination of the water deuterium fractionation ratios is particularly suitable. Previous studies derived HDO/H2O ratios in the warm inner regions of low-mass protostars. We here report a detection of the D2O 1(1,0)-1(0,1) transition toward the low-mass protostar NGC 1333 IRAS2A with the Plateau de Bure interferometer: this represents the first interferometric detection of D2O-and only the second solar-type protostar for which this isotopologue is detected. Using the observations of the HDO 5(4,2)-6(3,3) transition simultaneously detected and three other HDO lines previously observed, we show that the HDO line fluxes are well reproduced with a single excitation temperature of 218 +/- 21 K and a source size of similar to 0 ''.5. The D2O/HDO ratio is similar to(1.2 +/- 0.5) x 10(-2), while the use of previous (H2O)-O-18 observations give an HDO/H2O ratio of similar to(1.7 +/- 0.8) x 10(-3), i.e., a factor of seven lower than the D2O/HDO ratio. These results contradict the predictions of current grain surface chemical models and indicate that either the surface deuteration processes are poorly understood or that both sublimation of grain mantles and water formation at high temperatures (greater than or similar to 230 K) take place in the inner regions of this source. In the second scenario, the thermal desorption of the grain mantles would explain the high D2O/HDO ratio, while water formation at high temperature would explain significant extra production of H2O leading to a decrease of the HDO/H2O ratio.
C1 [Coutens, A.; Jorgensen, J. K.] Univ Copenhagen, Niels Bohr Inst, DK-2100 Copenhagen O, Denmark.
[Coutens, A.; Jorgensen, J. K.] Univ Copenhagen, Ctr Star & Planet Format, Nat Hist Museum Denmark, DK-1350 Copenhagen K, Denmark.
[Persson, M. V.; van Dishoeck, E. F.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands.
[van Dishoeck, E. F.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany.
[Vastel, C.] Univ Toulouse, UPS OMP, IRAP, F-31062 Toulouse, France.
[Vastel, C.] IRAP, CNRS, F-31028 Toulouse 4, France.
[Taquet, V.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20770 USA.
RP Coutens, A (reprint author), Univ Copenhagen, Niels Bohr Inst, Juliane Maries Vej 30, DK-2100 Copenhagen O, Denmark.
EM acoutens@nbi.dk
RI Coutens, Audrey/M-4533-2014
OI Coutens, Audrey/0000-0003-1805-3920
FU INSU/CNRS (France); MPG (Germany); IGN (Spain)
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).
NR 36
TC 10
Z9 10
U1 3
U2 8
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 SEP 1
PY 2014
VL 792
IS 1
AR L5
DI 10.1088/2041-8205/792/1/L5
PG 5
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AO4KO
UT WOS:000341306900005
ER
PT J
AU Kelley, MSP
Farnham, TL
Bodewits, D
Tricarico, P
Farnocchia, D
AF Kelley, Michael S. P.
Farnham, Tony L.
Bodewits, Dennis
Tricarico, Pasquale
Farnocchia, Davide
TI A STUDY OF DUST AND GAS AT MARS FROM COMET C/2013 A1 (SIDING SPRING)
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE celestial mechanics; comets: individual (C/2013 A1 (Siding Spring));
meteorites, meteors, meteoroids; methods: numerical
ID NUCLEUS; ATMOSPHERE; EQUATIONS
AB Although the nucleus of comet C/2013 A1 (Siding Spring) will safely pass Mars in 2014 October, the dust in the coma and tail will more closely approach the planet. Using a dynamical model of comet dust, we estimate the impact fluence. Based on our nominal model no impacts are expected at Mars. Relaxing our nominal model's parameters, the fluence is no greater than similar to 10(-7) grains m(-2) for grain radii larger than 10 mu m. Mars-orbiting spacecraft are unlikely to be impacted by large dust grains, but Mars may receive as many as similar to 10(7) grains, or similar to 100 kg of total dust. We also estimate the flux of impacting gas molecules commonly observed in comet comae.
C1 [Kelley, Michael S. P.; Farnham, Tony L.; Bodewits, Dennis] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Tricarico, Pasquale] Planetary Sci Inst, Tucson, AZ 85719 USA.
[Farnocchia, Davide] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Kelley, MSP (reprint author), Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
EM msk@astro.umd.edu
OI Kelley, Michael/0000-0002-6702-7676; Bodewits,
Dennis/0000-0002-2668-7248
FU University of Maryland by the NASA JPL Mars Critical Data Products
Program
FX This research was supported by a contract to the University of Maryland
by the NASA JPL Mars Critical Data Products Program.
NR 25
TC 15
Z9 15
U1 0
U2 3
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 SEP 1
PY 2014
VL 792
IS 1
AR L16
DI 10.1088/2041-8205/792/1/L16
PG 6
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AO4KO
UT WOS:000341306900016
ER
PT J
AU Pereira, TMD
De Pontieu, B
Carlsson, M
Hansteen, V
Tarbell, TD
Lemen, J
Title, A
Boerner, P
Hurlburt, N
Wulser, JP
Martinez-Sykora, J
Kleint, L
Golub, L
McKillop, S
Reeves, KK
Saar, S
Testa, P
Tian, H
Jaeggli, S
Kankelborg, C
AF Pereira, T. M. D.
De Pontieu, B.
Carlsson, M.
Hansteen, V.
Tarbell, T. D.
Lemen, J.
Title, A.
Boerner, P.
Hurlburt, N.
Wuelser, J. P.
Martinez-Sykora, J.
Kleint, L.
Golub, L.
McKillop, S.
Reeves, K. K.
Saar, S.
Testa, P.
Tian, H.
Jaeggli, S.
Kankelborg, C.
TI AN INTERFACE REGION IMAGING SPECTROGRAPH FIRST VIEW ON SOLAR SPICULES
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE Sun: atmosphere; Sun: chromosphere; Sun: transition region
ID OPTICAL TELESCOPE; II SPICULES; K LINES; MG II; IRIS; DYNAMICS; HINODE;
CHROMOSPHERE; MISSION; EVENTS
AB Solar spicules have eluded modelers and observers for decades. Since the discovery of the more energetic type II, spicules have become a heated topic but their contribution to the energy balance of the low solar atmosphere remains unknown. Here we give a first glimpse of what quiet-Sun spicules look like when observed with NASA's recently launched Interface Region Imaging Spectrograph (IRIS). Using IRIS spectra and filtergrams that sample the chromosphere and transition region, we compare the properties and evolution of spicules as observed in a coordinated campaign with Hinode and the Atmospheric Imaging Assembly. Our IRIS observations allow us to follow the thermal evolution of type II spicules and finally confirm that the fading of Ca II H spicules appears to be caused by rapid heating to higher temperatures. The IRIS spicules do not fade but continue evolving, reaching higher and falling back down after 500-800 s. Ca II H type II spicules are thus the initial stages of violent and hotter events that mostly remain invisible in Ca II H filtergrams. These events have very different properties from type I spicules, which show lower velocities and no fading from chromospheric passbands. The IRIS spectra of spicules show the same signature as their proposed disk counterparts, reinforcing earlier work. Spectroheliograms from spectral rasters also confirm that quiet-Sun spicules originate in bushes from the magnetic network. Our results suggest that type II spicules are indeed the site of vigorous heating (to at least transition region temperatures) along extensive parts of the upward moving spicular plasma.
C1 [Pereira, T. M. D.; De Pontieu, B.; Carlsson, M.; Hansteen, V.] Univ Oslo, Inst Theoret Astrophys, POB 1029, NO-0315 Oslo, Norway.
[De Pontieu, B.; Tarbell, T. D.; Lemen, J.; Title, A.; Boerner, P.; Hurlburt, N.; Wuelser, J. P.; Martinez-Sykora, J.; Kleint, L.] Lockheed Martin Solar & Astrophys Lab, Palo Alto, CA 94304 USA.
[Martinez-Sykora, J.; Kleint, L.] Bay Area Environm Res Inst, Sonoma, CA 95476 USA.
[Kleint, L.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Golub, L.; McKillop, S.; Reeves, K. K.; Saar, S.; Testa, P.; Tian, H.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Jaeggli, S.; Kankelborg, C.] Montana State Univ, Dept Phys, Bozeman, MT 59717 USA.
RP Pereira, TMD (reprint author), Univ Oslo, Inst Theoret Astrophys, POB 1029, NO-0315 Oslo, Norway.
EM tiago.pereira@astro.uio.no
RI Reeves, Katharine/P-9163-2014
FU NSC (Norway); European Research Council [291058]; NASA [NNM07AA01C,
NNG09FA40C]
FX IRIS is a NASA Small Explorer mission developed and operated by LMSAL
with mission operations executed at NASA ARC and major contributions to
downlink communications funded by the NSC (Norway). Hinode is a Japanese
mission developed by ISAS/JAXA, with the NAOJ as domestic partner and
NASA and STFC (UK) as international partners. It is operated in
cooperation with ESA and NSC (Norway). This work was supported by the
European Research Council grant No. 291058 and by NASA under contracts
NNM07AA01C (Hinode), and NNG09FA40C (IRIS).
NR 30
TC 27
Z9 27
U1 0
U2 2
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 SEP 1
PY 2014
VL 792
IS 1
AR L15
DI 10.1088/2041-8205/792/1/L15
PG 6
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AO4KO
UT WOS:000341306900015
ER
PT J
AU Landerer, FW
Gleckler, PJ
Lee, T
AF Landerer, Felix W.
Gleckler, Peter J.
Lee, Tong
TI Evaluation of CMIP5 dynamic sea surface height multi-model simulations
against satellite observations
SO CLIMATE DYNAMICS
LA English
DT Article
DE Sea surface height; CMIP5; GCM skill; Model evaluation; AR5
ID OCEAN CIRCULATION; CLIMATE MODELS; LEVEL CHANGE; VARIABILITY;
ATTRIBUTION; PROJECTIONS; PRODUCTS; IMPACT; RISE; FLUX
AB We evaluate the representation of dynamic sea surface height (SSH) fields of 33 global coupled models (GCMs) contributed to the fifth phase of the Coupled Model Intercomparison Project (CMIP5). We use observations from satellite altimetry and basic performance metrics to quantify the ability of the GCMs to replicate observed SSH of the time-mean, seasonal cycle, and inter-annual variability patterns. The time-mean SSH representation has markedly improved from CMIP3 to CMIP5, both in terms of overall reduction in root-mean square differences, and in terms of reduced GCM ensemble spread. Biases of the time-mean SSH field in the Indian and Pacific Ocean equatorial regions are consistent with biases in the zonal surface wind stress fields identified with independent measurements. In the Southern Ocean, the latitude of the maximum meridional gradient of the zonal mean SSH CMIP5 models is shifted equatorward, consistent with the GCMs' spatial biases in the maximum of the zonal mean westerly surface wind stress fields. However, while the Southern Ocean SSH gradients correlate well with the maximum Antarctic circumpolar current transports, there is no significant correlation with the maximum zonal mean wind stress amplitudes, consistent with recent findings that the eddy parameterisations in GCMs dominate over wind stress amplitudes in this region. There is considerable spread across the CMIP5 ensemble for the seasonal and interannual SSH variability patterns. Because of the short observational period, the interannual variability patterns depend on the time-period over which they are derived, while no such dependency is found for the time-mean patterns. The model performance metrics for SSH presented here provide insight into GCM shortcoming due to inadequate model physics or processes. While the diagnostics of CMIP5 GCM performance relative to observations reveal that some models are clearly better than others, model performance is sensitive to the spatio-temporal scales chosen.
C1 [Landerer, Felix W.; Lee, Tong] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
[Gleckler, Peter J.] Lawrence Livermore Natl Lab, Program Climate Model Diag & Intercomparison, Livermore, CA USA.
RP Landerer, FW (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
EM felix.w.landerer@jpl.nasa.gov
OI Landerer, Felix/0000-0003-2678-095X
FU NASA
FX We acknowledge the GCM modeling groups, the PCMDI, and the WCRP's
Working Group on Coupled Modeling for their roles in making available
the WCRP CMIP3 and CMIP5 multimodel data sets. Support of these data
sets is provided by the Office of Science, US Department of Energy.
FWL's and TL's work was performed at the Jet Propulsion Laboratory,
California Institute of Technology, under contract with NASA.
NR 47
TC 9
Z9 9
U1 1
U2 20
PU SPRINGER
PI NEW YORK
PA 233 SPRING ST, NEW YORK, NY 10013 USA
SN 0930-7575
EI 1432-0894
J9 CLIM DYNAM
JI Clim. Dyn.
PD SEP
PY 2014
VL 43
IS 5-6
BP 1271
EP 1283
DI 10.1007/s00382-013-1939-x
PG 13
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA AO5FR
UT WOS:000341369700008
ER
PT J
AU Boussaha, F
Kawamura, J
Stern, J
Jung-Kubiak, C
AF Boussaha, Faouzi
Kawamura, Jonathan
Stern, Jeffery
Jung-Kubiak, Cecile
TI 2.7 THz Balanced Waveguide HEB Mixer
SO IEEE TRANSACTIONS ON TERAHERTZ SCIENCE AND TECHNOLOGY
LA English
DT Article
DE Heterodyne detection; hot electron bolometer; hybrid coupler; silicon
micromachining; terahertz (THz) frequency; waveguide
ID SIS MIXER
AB We report on the development of a waveguide-based balanced superconducting mixer for operation near 2.7 THz. The mixer employs a pair of NbN hot-electron bolometers defined on 6 mu m-thick silicon substrate that follows a 90 degrees hybrid coupler. To produce the critical structures of the coupler and waveguide embedding circuit, we have utilized silicon micromachining techniques based on deep reactive ion etching. Operating near 4.2 K bath temperature, we have measured a minimum uncorrected DSB receiver noise temperature of less than 2000 K using Callen-Welton formula and local oscillator sideband noise rejection better than 13 +/- 3 dB at 2.74 THz. The concept is suitable for building arrays, readily scalable for higher frequencies up 5 THz, and could accommodate other mixer technologies, such as room-temperature Schottky diode mixers.
C1 [Boussaha, Faouzi; Kawamura, Jonathan; Stern, Jeffery; Jung-Kubiak, Cecile] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Boussaha, Faouzi] Observ Paris, LERMA CNRS UMR 8112, F-75014 Paris, France.
RP Boussaha, F (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
EM Jonathan.h.kawamura@jpl.nasa.gov
FU Jet Propulsion Laboratory, California Institute of Technology; Oak Ridge
Associated Universities through the NASA Postdoctoral Program (NPP);
National Aeronautics and Space Administration
FX This work was supported in part by the Jet Propulsion Laboratory,
California Institute of Technology, under a contract with the National
Aeronautics and Space Administration, and partly supported by the Oak
Ridge Associated Universities through the NASA Postdoctoral Program
(NPP).
NR 24
TC 8
Z9 8
U1 4
U2 22
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 SEP
PY 2014
VL 4
IS 5
BP 545
EP 551
DI 10.1109/TTHZ.2014.2342507
PG 7
WC Engineering, Electrical & Electronic; Optics; Physics, Applied
SC Engineering; Optics; Physics
GA AO7YQ
UT WOS:000341569400004
ER
PT J
AU Leal-Sevillano, CA
Reck, TJ
Chattopadhyay, G
Ruiz-Cruz, JA
Montejo-Garai, JR
Rebollar, JM
AF Leal-Sevillano, Carlos A.
Reck, Theodore J.
Chattopadhyay, Goutam
Ruiz-Cruz, Jorge A.
Montejo-Garai, Jose R.
Rebollar, Jesus M.
TI Development of a Wideband Compact Orthomode Transducer for the 180-270
GHz Band
SO IEEE TRANSACTIONS ON TERAHERTZ SCIENCE AND TECHNOLOGY
LA English
DT Article
DE Orthomode transducer; terahertz; waveguide; wideband
AB In this paper, we report the development of a wideband compact orthomode transducer (OMT) for the 180-270 GHz band. The OMT design is based on the classical high performance Boifot waveguide junction and implemented in split-block using high precision CNC milling. The obtained results validate the high performance operation in a 40% fractional bandwidth and constitute a remarkable achievement at this high frequency band.
C1 [Leal-Sevillano, Carlos A.; Montejo-Garai, Jose R.; Rebollar, Jesus M.] Univ Politecn Madrid, ETSI Telecomunicac, Dept Electromagnetismo & Teoria Circuitos, E-28040 Madrid, Spain.
[Reck, Theodore J.; Chattopadhyay, Goutam] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Ruiz-Cruz, Jorge A.] Univ Autonoma Madrid, Escuela Politecn Super, E-28049 Madrid, Spain.
RP Leal-Sevillano, CA (reprint author), Univ Politecn Madrid, ETSI Telecomunicac, Dept Electromagnetismo & Teoria Circuitos, E-28040 Madrid, Spain.
EM caleal@etc.upm.es
RI Ruiz-Cruz, Jorge/C-8159-2014
OI Ruiz-Cruz, Jorge/0000-0003-3909-8263
FU Jet Propulsion Laboratory, California Institute of Technology, Pasadena,
CA; National Aeronautics and Space Administration; Spanish government
program [TEC2010-17795]; CONSOLIDER [CSD2008-00068]; Universidad
Politecnica de Madrid
FX This work was supported by the Jet Propulsion Laboratory, California
Institute of Technology, Pasadena, CA, under a contract with the
National Aeronautics and Space Administration. This work was supported
in part by the Spanish government program under TEC2010-17795, by
CONSOLIDER under CSD2008-00068, and by the Universidad Politecnica de
Madrid under a Ph.D. grant.
NR 10
TC 4
Z9 4
U1 1
U2 5
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 SEP
PY 2014
VL 4
IS 5
BP 634
EP 636
DI 10.1109/TTHZ.2014.2336540
PG 3
WC Engineering, Electrical & Electronic; Optics; Physics, Applied
SC Engineering; Optics; Physics
GA AO7YQ
UT WOS:000341569400017
ER
PT J
AU Hurwitz, FI
Gallagher, M
Olin, TC
Shave, MK
Ittes, MA
Olafson, KN
Fields, MG
Rogers, RB
Guo, HQ
AF Hurwitz, Frances I.
Gallagher, Meghan
Olin, Tracy C.
Shave, Molly K.
Ittes, Marlyssa A.
Olafson, Katy N.
Fields, Meredith G.
Rogers, Richard B.
Guo, Haiquan
TI Optimization of Alumina and Aluminosilicate Aerogel Structure for
High-Temperature Performance
SO INTERNATIONAL JOURNAL OF APPLIED GLASS SCIENCE
LA English
DT Article
ID SOL-GEL PROCESS; MULLITE; PHASE; NMR; PRECURSORS; SYSTEM; AL-27;
HYDROLYSIS; ALKOXIDES; XEROGELS
AB Alumina and aluminosilicate aerogels offer potential for use at temperatures above 700 degrees C, where silica aerogels begin to sinter. Stability of alumina and aluminosilicate pore structures at high temperatures is governed by the starting aerogel structure, which, in turn is controlled by the synthesis route. Structure, morphology, and crystallization behavior are compared for aerogels synthesized from AlCl3 and propylene oxide with those synthesized from a variety of boehmite precursors. The aerogels possessing a crystalline boehmite structure in the as-synthesized condition retained mesoporous structures to temperatures of 1200 degrees C, while the AlCl3-derived aerogels, although exhibiting higher as-synthesized surface areas, crystallized and densified at 980-1005 degrees C.
C1 [Hurwitz, Frances I.; Gallagher, Meghan; Olin, Tracy C.; Shave, Molly K.; Ittes, Marlyssa A.; Olafson, Katy N.; Fields, Meredith G.; Rogers, Richard B.] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA.
[Guo, Haiquan] Ohio Aerosp Inst, Cleveland, OH 44135 USA.
RP Hurwitz, FI (reprint author), NASA, Glenn Res Ctr, Cleveland, OH 44135 USA.
EM frances.hurwitz@nasa.gov
FU NASA Aeronautics Research and Space Technology Mission Directorates;
Radioisotope Power Systems Program; NASA USRP; NASA LERCIP
FX The authors wish to acknowledge the late Anna R. Palczer of NASA Glenn
Research Center for her many contributions to this work. We wish to
thank Dr. Matthew P. Espe and Anna M. Reinsel of the University of Akron
for the NMR characterization, Derek F. Johnson of NASA Glenn Research
Center for thermal and elemental analysis, and Michael T. Cox of NASA
Glenn Research Center for XRD. Thanks as well to Sasol N. A. for
donation of the boehmite powders. We also wish to acknowledge funding
support from the NASA Aeronautics Research and Space Technology Mission
Directorates, the Radioisotope Power Systems Program, and the NASA USRP
and LERCIP student internship programs.
NR 36
TC 6
Z9 6
U1 7
U2 40
PU WILEY PERIODICALS, INC
PI SAN FRANCISCO
PA ONE MONTGOMERY ST, SUITE 1200, SAN FRANCISCO, CA 94104 USA
SN 2041-1286
EI 2041-1294
J9 INT J APPL GLASS SCI
JI Int. J. Appl. Glass Sci.
PD SEP
PY 2014
VL 5
IS 3
SI SI
BP 276
EP 286
DI 10.1111/ijag.12070
PG 11
WC Materials Science, Ceramics
SC Materials Science
GA AO9GG
UT WOS:000341663500008
ER
PT J
AU Kim, JH
Ou, ML
Park, JD
Morris, KR
Schwaller, MR
Wolff, DB
AF Kim, Ji-Hye
Ou, Mi-Lim
Park, Jun-Dong
Morris, Kenneth R.
Schwaller, Mathew R.
Wolff, David B.
TI Global Precipitation Measurement (GPM) Ground Validation (GV) Prototype
in the Korean Peninsula
SO JOURNAL OF ATMOSPHERIC AND OCEANIC TECHNOLOGY
LA English
DT Article
ID MEASURING MISSION TRMM; LATENT HEATING DISTRIBUTIONS; RAIN-GAUGE
MEASUREMENTS; RADAR OBSERVATIONS; MICROWAVE IMAGER; SPACEBORNE RADAR;
SATELLITE; CALIBRATION; ALGORITHMS; VERSION-6
AB Since 2009, the Korea Meteorological Administration (KMA) has participated in ground validation (GV) projects through international partnerships within the framework of the Global Precipitation Measurement (GPM) Mission. The goal of this work is to assess the reliability of ground-based measurements in the Korean Peninsula as a means for validating precipitation products retrieved from satellite microwave sensors, with an emphasis on East Asian precipitation. KMA has a well-developed operational weather service infrastructure composed of meteorological radars, a dense rain gauge network, and automated weather stations. Measurements from these systems, including data from four ground-based radars (GRs), were combined with satellite data from the Tropical Rainfall Measuring Mission (TRMM) precipitation radar (PR) and used as a proxy for GPM GV over the Korean Peninsula. A time series of mean reflectivity differences (GR-PR) for stratiform-only and above-brightband-only data showed that the time-averaged difference fell between -2.0 and +1.0 dBZ for the four GRs used in this study. Site-specific adjustments for these relative mean biases were applied to GR reflectivities, and detailed statistical comparisons of reflectivity and rain rate between PR and bias-adjusted GR were carried out. In rain-rate comparisons, surface rain from the TRMM Microwave Imager (TMI) and the rain gauges were added and the results varied according to rain type. Bias correction has had a positive effect on GR rain rate comparing with PR and gauge rain rates. This study confirmed advance preparation for GPM GV system was optimized on the Korean Peninsula using the official framework.
C1 [Kim, Ji-Hye; Ou, Mi-Lim] Korea Meteorol Adm, Natl Inst Meteorol Res, Seogwipo Si 697845, Jeju Do, South Korea.
[Kim, Ji-Hye] Yonsei Univ, Dept Atmospher Sci, Seoul 120749, South Korea.
[Park, Jun-Dong] Korea Meteorol Adm, Natl Meteorol Satellite Ctr, Jincheon, South Korea.
[Park, Jun-Dong] Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20742 USA.
[Morris, Kenneth R.; Schwaller, Mathew R.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Wolff, David B.] NASA, Wallops Flight Facil, Wallops Isl, VA USA.
RP Ou, ML (reprint author), Korea Meteorol Adm, Natl Inst Meteorol Res, 33 Seohobuk Ro, Seogwipo Si 697845, Jeju Do, South Korea.
EM milim@korea.kr
RI Measurement, Global/C-4698-2015
FU Research for the Meteorological and Earthquake Observation Technology
and Its Application of the National Institute of Meteorological
Research, Korea Meteorological Administration (KMA), South Korea
FX This study was supported by the Research for the Meteorological and
Earthquake Observation Technology and Its Application of the National
Institute of Meteorological Research, Korea Meteorological
Administration (KMA), South Korea. The authors thank the NASA Goddard
Space Flight Center (GSFC) for providing data processing software for
the GPM Ground Validation System (GVS) and TRMM products.
NR 44
TC 1
Z9 2
U1 0
U2 13
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 SEP
PY 2014
VL 31
IS 9
BP 1902
EP 1921
DI 10.1175/JTECH-D-13-00193.1
PG 20
WC Engineering, Ocean; Meteorology & Atmospheric Sciences
SC Engineering; Meteorology & Atmospheric Sciences
GA AO4WM
UT WOS:000341342100004
ER
PT J
AU Song, H
Lin, WY
Lin, YL
Wolf, AB
Donner, LJ
Del Genio, AD
Neggers, R
Endo, S
Liu, YG
AF Song, Hua
Lin, Wuyin
Lin, Yanluan
Wolf, Audrey B.
Donner, Leo J.
Del Genio, Anthony D.
Neggers, Roel
Endo, Satoshi
Liu, Yangang
TI Evaluation of Cloud Fraction Simulated by Seven SCMs against the ARM
Observations at the SGP Site
SO JOURNAL OF CLIMATE
LA English
DT Article
ID SINGLE-COLUMN MODELS; RADIATION MEASUREMENT PROGRAM; GENERAL-CIRCULATION
MODELS; SHALLOW CUMULUS CONVECTION; PHASE ARCTIC CLOUD; LARGE-SCALE
MODELS; CLIMATE MODELS; SURFACE OBSERVATIONS; PARAMETERIZATION; SYSTEM
AB This study evaluates the performances of seven single-column models (SCMs) by comparing simulated cloud fraction with observations at the Atmospheric Radiation Measurement Program (ARM) Southern Great Plains (SGP) site from January 1999 to December 2001. Compared with the 3-yr mean observational cloud fraction, the ECMWF SCM underestimates cloud fraction at all levels and the GISS SCM underestimates cloud fraction at levels below 200 hPa. The two GFDL SCMs underestimate lower-to-middle level cloud fraction but overestimate upper-level cloud fraction. The three Community Atmosphere Model (CAM) SCMs overestimate upper-level cloud fraction and produce lower-level cloud fraction similar to the observations but as a result of compensating overproduction of convective cloud fraction and underproduction of stratiform cloud fraction. Besides, the CAM3 and CAM5 SCMs both overestimate midlevel cloud fraction, whereas the CAM4 SCM underestimates. The frequency and partitioning analyses show a large discrepancy among the seven SCMs: Contributions of nonstratiform processes to cloud fraction production are mainly in upper-level cloudy events over the cloud cover range 10%-80% in SCMs with prognostic cloud fraction schemes and in lower-level cloudy events over the cloud cover range 15%-50% in SCMs with diagnostic cloud fraction schemes. Further analysis reveals different relationships between cloud fraction and relative humidity (RH) in the models and observations. The underestimation of lower-level cloud fraction in most SCMs is mainly due to the larger threshold RH used in models. The overestimation of upper-level cloud fraction in the three CAM SCMs and two GFDL SCMs is primarily due to the overestimation of RH and larger mean cloud fraction of cloudy events plus more occurrences of RH around 40%-80%, respectively.
C1 [Song, Hua; Lin, Wuyin; Endo, Satoshi; Liu, Yangang] Brookhaven Natl Lab, Upton, NY 11973 USA.
[Lin, Yanluan] Tsinghua Univ, Ctr Earth Syst Sci, Key Lab Earth Syst Modeling, Minist Educ, Beijing 100084, Peoples R China.
[Wolf, Audrey B.] Columbia Univ, New York, NY USA.
[Donner, Leo J.] NOAA, Geophys Fluid Dynam Lab, Princeton, NJ USA.
[Del Genio, Anthony D.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
[Neggers, Roel] Royal Netherlands Meteorol Inst, NL-3730 AE De Bilt, Netherlands.
RP Song, H (reprint author), Brookhaven Natl Lab, Div Atmospher Sci, 75 Rutherford Dr,Bldg 815E, Upton, NY 11973 USA.
EM hsong@bnl.gov
RI lin, yanluan/A-6333-2015; Liu, Yangang/H-6154-2011
FU Office of Biological and Environmental Research of the U.S. Department
of Energy as part of the Earth Systems Modeling (ESM) program via the
FASTER project; Atmospheric System Research program; NASA Modeling and
Analysis Program
FX This work is supported by the Office of Biological and Environmental
Research of the U.S. Department of Energy as part of the Earth Systems
Modeling (ESM) program via the FASTER project
(http://www.bnl.gov/faster) and Atmospheric System Research program. Del
Genio is supported also by the NASA Modeling and Analysis Program. We
thank Editor Dr. Robert Wood and three anonymous reviewers for their
insightful and constructive comments. We also thank Dr. Stephen Schwartz
for his interest and helpful suggestions.
NR 61
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
EI 1520-0442
J9 J CLIMATE
JI J. Clim.
PD SEP 1
PY 2014
VL 27
IS 17
BP 6698
EP 6719
DI 10.1175/JCLI-D-13-00555.1
PG 22
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA AO4BS
UT WOS:000341281800021
ER
PT J
AU Shindell, D
AF Shindell, Drew
TI Reply to 'Questions of bias in climate models'
SO NATURE CLIMATE CHANGE
LA English
DT Letter
C1 NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
RP Shindell, D (reprint author), NASA, Goddard Inst Space Studies, 2880 Broadway, New York, NY 10025 USA.
EM drew.shindell@duke.edu
RI Shindell, Drew/D-4636-2012
NR 6
TC 2
Z9 2
U1 0
U2 13
PU NATURE PUBLISHING GROUP
PI LONDON
PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND
SN 1758-678X
EI 1758-6798
J9 NAT CLIM CHANGE
JI Nat. Clim. Chang.
PD SEP
PY 2014
VL 4
IS 9
BP 742
EP 743
PG 3
WC Environmental Sciences; Environmental Studies; Meteorology & Atmospheric
Sciences
SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences
GA AO7YS
UT WOS:000341569700005
ER
PT J
AU Badavi, FF
Walker, SA
Koos, LMS
AF Badavi, Francis F.
Walker, Steven A.
Koos, Lindsey M. Santos
TI Evaluation of the new radiation belt AE9/AP9/SPM model for a cislunar
mission
SO ACTA ASTRONAUTICA
LA English
DT Article
DE Trapped radiation belts; Cislunar space; Lagrange point L2; Effective
dose
ID ADULT VOXEL PHANTOM; PROTECTION DOSIMETRY
AB Space mission planners continue to experience challenges associated with human space flight. Concerned with the omnipresence of harmful ionizing radiation in space, at the mission design stage, mission planners must evaluate the amount of exposure the crew of a spacecraft is subjected to during the transit trajectory from low Earth orbit (LEO) to geosynchronous orbit (GEO) and beyond (free space). The Earth's geomagnetic field is located within the domain of LEO-GEO and, depending on latitude, extends out some 40,000-60,000 km. This field contains the Van Allen trapped electrons, protons, and low-energy plasmas, such as the nuclei of hydrogen, helium, oxygen, and to a lesser degree other atoms. In addition, there exist the geomagnetically attenuated energetic galactic cosmic rays (GCR). These particles are potentially harmful to improperly shielded crew members and onboard subsystems. Mitigation strategies to limit the exposure due to free space GCR and sporadic solar energetic particles (SEP) such as flare and coronal mass ejection (CME) must also be exercised beyond the trapped field. Presented in this work is the exposure analysis for a multi-vehicle mission planned for the epoch of February 2020 from LEO to the Earth-moon Lagrange-point two (L2), located approximately 63,000 km beyond the orbit of the Earth-moon binary system. Space operation at 12 provides a gravitationally stable orbit for a vehicle and partially eliminates the need for periodic thrust-vectoring to maintain orbital stability. In the cislunar (Earth-moon) space of L2, the mission trajectory and timeline in this work call for a cargo vehicle to rendezvous with a crew vehicle. This is followed by 15 days of space activities at 12 while the cargo and crew vehicles are docked after which the crew returns to Earth. The mission epoch of 2020 is specifically chosen as it is anticipated that the next solar minimum (i.e. end of cycle 24) in the Sun's approximate 11 years cycle will take place around this time. From a mission planning point of view, this date is ideal as the predictable GCR exposure will be at a maximum, while the sporadic SEP will be at a minimum. In addition, it is anticipated that by 2020 a vehicle capable of launching a crew of four will be operationally ready. During the LEO-GEO transit, the crew and cargo vehicles will encounter exposure from trapped particles and attenuated GCR, followed by free space exposure due to GCR and SEP during solar active times. Within the trapped field, a challenge arises from properly calculating the amount of exposure acquired. Within this field, in the absence of SEP (i.e. solar quiet times), the vehicles will have to transit through an inner proton belt, an inner and outer electron belts, and an attenuated GCR field. There exist a number of models to define the intensities of the trapped particles during the quiet and active SEP. Among the more established trapped models are the historic and popular electron/proton AE8/AP8 model dating back to the 1980s, the historic and less popular electron/proton CRRES model dating back to 1990s, and the recently released electron/proton/space plasma AE9/AP9/SPM model. The AE9/AP9/SPM model is a major improvement over the older AE8/AP8 and CRRES models. This model is derived from numerous measurements acquired over four solar cycles dating back to the 1970s, roughly representing 40 years of data collection. In contrast, the older AE8/AP8 and CRRES models were limited to only a few months of measurements taken during the prior solar minima and maxima.
In this work, within the trapped field, along the design trajectory of the crew vehicle, the AE9/AP9/SPM model is evaluated against the older AE8/AP8 model during solar quiet times. The analysis is then extended to the GCR dominated en-route, cislunar L2 space and return trajectories in order to provide cumulative exposure estimates to the crew vehicle for the duration of the entire mission. (C) 2014 IAA. Published by Elsevier Ltd. All rights reserved.
C1 [Badavi, Francis F.; Walker, Steven A.; Koos, Lindsey M. Santos] Old Dominion Univ, Norfolk, VA 23529 USA.
RP Badavi, FF (reprint author), NASA, Langley Res Ctr, MS 188E, Hampton, VA 23681 USA.
EM francis.f.badavi@nasa.gov
FU NASA Human Research Program (HRP) under the Human Exploration and
Operations Mission Directorate; NASA [NNX12AN58A, NNX09AR20A]
FX The authors wish to express their gratitude to Garry Qualls of LaRC for
providing the CEV604 crew vehicle geometry; Jonathan Chrone of
Analytical Mechanics Associates (AMA) Inc. for providing the epoch
specific cislunar trajectory; W.R. Johnston of Space Vehicles
Directorate, Air Force Research Laboratory, Kirtland AFB and T.P.
O'Brien of Aerospace Corporation for assistance with the AE9/AP9/SPM
trapped model. This work was supported by the NASA Human Research
Program (HRP) under the Human Exploration and Operations Mission
Directorate, and partially by the NASA Grants NNX12AN58A and NNX09AR20A.
NR 27
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U1 1
U2 11
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0094-5765
EI 1879-2030
J9 ACTA ASTRONAUT
JI Acta Astronaut.
PD SEP-OCT
PY 2014
VL 102
BP 156
EP 168
DI 10.1016/j.actaastro.2014.06.008
PG 13
WC Engineering, Aerospace
SC Engineering
GA AN6HB
UT WOS:000340694500014
ER
PT J
AU Kakoi, M
Howell, KC
Folta, D
AF Kakoi, Masaki
Howell, Kathleen C.
Folta, David
TI Access to Mars from Earth-Moon libration point orbits: Manifold and
direct options
SO ACTA ASTRONAUTICA
LA English
DT Article; Proceedings Paper
CT 64th International Astronautical Congress (IAC)
CY SEP 23-27, 2013
CL Beijing, PEOPLES R CHINA
DE Multi-body dynamics; Circular restricted three-body problem; Invariant
manifolds; Libration point orbits; System-to-system transfer; Mars
ID DYNAMICAL-SYSTEMS THEORY; INVARIANT-MANIFOLDS; SUN-EARTH; TRANSFERS;
DESIGN; TRAJECTORIES; MISSION; CAPTURE; ESCAPE
AB This investigation is focused specifically on transfers from Earth-Moon L-1/L-2 libration point orbits to Mars. Initially, the analysis is based on the circular restricted three-body problem to utilize the framework of the invariant manifolds. Various departure scenarios are compared, including arcs that leverage manifolds associated with the Sun-Earth L-2 orbits as well as non-manifold trajectories. For the manifold options, ballistic transfers from Earth-Moon L-2 libration point orbits to Sun-Earth L-1/L-2 halo orbits are first computed. This autonomous procedure applies to both departure and arrival between the Earth-Moon and Sun-Earth systems. Departure times in the lunar cycle, amplitudes and types of libration point orbits, manifold selection, and the orientation/location of the surface of section all contribute to produce a variety of options. As the destination planet, the ephemeris position for Mars is employed throughout the analysis. The complete transfer is transitioned to the ephemeris model after the initial design phase. Results for multiple departure/arrival scenarios are compared. (C) 2014 IAA. Published by Elsevier Ltd. All rights reserved.
C1 [Kakoi, Masaki; Howell, Kathleen C.] Purdue Univ, Sch Aeronaut & Astronaut, W Lafayette, IN 47907 USA.
[Folta, David] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Kakoi, M (reprint author), Purdue Univ, Sch Aeronaut & Astronaut, 701 W Stadium Ave, W Lafayette, IN 47907 USA.
EM kakoi@purdue.edu; howell@purdue.edu; david.c.folta@nasa.gov
OI Howell, Kathleen/0000-0002-1298-5017
NR 42
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PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0094-5765
EI 1879-2030
J9 ACTA ASTRONAUT
JI Acta Astronaut.
PD SEP-OCT
PY 2014
VL 102
BP 269
EP 286
DI 10.1016/j.actaastro.2014.06.010
PG 18
WC Engineering, Aerospace
SC Engineering
GA AN6HB
UT WOS:000340694500025
ER
PT J
AU Clegg, SM
Wiens, R
Misra, AK
Sharma, SK
Lambert, J
Bender, S
Newell, R
Nowak-Lovato, K
Smrekar, S
Dyar, MD
Maurice, S
AF Clegg, Samuel M.
Wiens, Roger
Misra, Anupam K.
Sharma, Shiv K.
Lambert, James
Bender, Steven
Newell, Raymond
Nowak-Lovato, Kristy
Smrekar, Sue
Dyar, M. Darby
Maurice, Sylvestre
TI Planetary Geochemical Investigations Using Raman and Laser-Induced
Breakdown Spectroscopy
SO APPLIED SPECTROSCOPY
LA English
DT Article
DE Raman spectroscopy; Laser-induced breakdown spectroscopy; LIBS; Mars
geology; Venus geology; Remote sensing
ID CHEMCAM INSTRUMENT SUITE; BULK AQUEOUS-SOLUTIONS; IN-SITU;
HIGH-PRESSURE; GALE CRATER; PIGMENT IDENTIFICATION; MARS; EXPLORATION;
SURFACES; SCIENCE
AB An integrated Raman spectroscopy and laser-induced breakdown spectroscopy (LIBS) instrument is a valuable geoanalytical tool for future planetary missions to Mars, Venus, and elsewhere. The Chem Cam instrument operating on the Mars Curiosity rover includes a remote LIBS instrument. An integrated Raman-LIBS spectrometer (RLS) based on the Chem Cam architecture could be used as a reconnaissance tool for other contact instruments as well as a primary science instrument capable of quantitative mineralogical and geochemical analyses. Replacing one of the Chem Cam spectrometers with a miniature transmission spectrometer enables a Raman spectroscopy mineralogical analysis to be performed, complementing the LIBS chemical analysis while retaining an overall architecture resembling Chem Cam. A prototype transmission spectrometer was used to record Raman spectra under both Martian and Venus conditions. Two different high-pressure and high-temperature cells were used to collect the Raman and LIBS spectra to simulate surface conditions on Venus. The resulting LIBS spectra were used to generate a limited partial least squares Venus calibration model for the major elements. These experiments demonstrate the utility and feasibility of a combined RLS instrument.
C1 [Clegg, Samuel M.; Wiens, Roger; Bender, Steven; Newell, Raymond; Nowak-Lovato, Kristy] Los Alamos Natl Lab, Los Alamos, NM 87545 USA.
[Misra, Anupam K.; Sharma, Shiv K.] Univ Hawaii Manoa, Hawaii Inst Geophys & Planetol, Honolulu, HI 96822 USA.
[Lambert, James; Smrekar, Sue] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Dyar, M. Darby] Mt Holyoke Coll, Dept Astron, S Hadley, MA 01075 USA.
[Maurice, Sylvestre] Univ Toulouse, Inst Rech Astrophys & Planetol, Toulouse 04, France.
RP Clegg, SM (reprint author), Los Alamos Natl Lab, POB 1663, Los Alamos, NM 87545 USA.
EM sclegg@lanl.gov
OI Clegg, Sam/0000-0002-0338-0948
FU LANL Laboratory Directed Research and Development (LORD) program; NASA
New Frontiers program; NASA Mars Science Laboratory program
FX We gratefully acknowledge the LANL Laboratory Directed Research and
Development (LORD) program, the NASA New Frontiers program, and the NASA
Mars Science Laboratory program for funding various aspects of the study
presented here. We also gratefully acknowledge David J. Cremers and Amy
J. Bauer for the gracious invitation to present at the SCIX conference
as well as the SCIX organizers for the opportunity to contribute to this
special issue.
NR 61
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PU SAGE PUBLICATIONS INC
PI THOUSAND OAKS
PA 2455 TELLER RD, THOUSAND OAKS, CA 91320 USA
SN 0003-7028
EI 1943-3530
J9 APPL SPECTROSC
JI Appl. Spectrosc.
PD SEP
PY 2014
VL 68
IS 9
BP 925
EP 936
DI 10.1366/13-07386
PG 12
WC Instruments & Instrumentation; Spectroscopy
SC Instruments & Instrumentation; Spectroscopy
GA AN8PF
UT WOS:000340865400003
PM 25226246
ER
PT J
AU Ade, PAR
Aikin, RW
Amiri, M
Barkats, D
Benton, SJ
Bischoff, CA
Bock, JJ
Brevik, JA
Buder, I
Bullock, E
Davis, G
Day, PK
Dowell, CD
Duband, L
Filippini, JP
Fliescher, S
Golwala, SR
Halpern, M
Hasselfield, M
Hildebrandt, SR
Hilton, GC
Irwin, KD
Karkare, KS
Kaufman, JP
Keating, BG
Kernasovskiy, SA
Kovac, JM
Kuo, CL
Leitch, EM
Llombart, N
Lueker, M
Netterfield, CB
Nguyen, HT
O'Brient, R
Ogburn, RW
Orlando, A
Pryke, C
Reintsema, CD
Richter, S
Schwarz, R
Sheehy, CD
Staniszewski, ZK
Story, KT
Sudiwala, RV
Teply, GP
Tolan, JE
Turner, AD
Vieregg, AG
Wilson, P
Wong, CL
Yoon, KW
AF Ade, P. A. R.
Aikin, R. W.
Amiri, M.
Barkats, D.
Benton, S. J.
Bischoff, C. A.
Bock, J. J.
Brevik, J. A.
Buder, I.
Bullock, E.
Davis, G.
Day, P. K.
Dowell, C. D.
Duband, L.
Filippini, J. P.
Fliescher, S.
Golwala, S. R.
Halpern, M.
Hasselfield, M.
Hildebrandt, S. R.
Hilton, G. C.
Irwin, K. D.
Karkare, K. S.
Kaufman, J. P.
Keating, B. G.
Kernasovskiy, S. A.
Kovac, J. M.
Kuo, C. L.
Leitch, E. M.
Llombart, N.
Lueker, M.
Netterfield, C. B.
Nguyen, H. T.
O'Brient, R.
Ogburn, R. W.
Orlando, A.
Pryke, C.
Reintsema, C. D.
Richter, S.
Schwarz, R.
Sheehy, C. D.
Staniszewski, Z. K.
Story, K. T.
Sudiwala, R. V.
Teply, G. P.
Tolan, J. E.
Turner, A. D.
Vieregg, A. G.
Wilson, P.
Wong, C. L.
Yoon, K. W.
CA Bicep2 Collaboration
TI BICEP2. II. EXPERIMENT AND THREE-YEAR DATA SET
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE cosmic background radiation; cosmology: observations; gravitational
waves; inflation; instrumentation: polarimeters; telescopes
ID TRANSITION-EDGE SENSORS; BACKGROUND POLARIZATION EXPERIMENTS; ANGULAR
SCALE POLARIZATION; POWER SPECTRA; GRAVITY-WAVES; SOUTH-POLE; MICROWAVE;
ANISOTROPY; RADIATION; PROBE
AB We report on the design and performance of the BICEP2 instrument and on its three-year data set. BICEP2 was designed to measure the polarization of the cosmic microwave background (CMB) on angular scales of 1 degrees-5 degrees(l = 40-200), near the expected peak of the B-mode polarization signature of primordial gravitational waves from cosmic inflation. Measuring B-modes requires dramatic improvements in sensitivity combined with exquisite control of systematics. The BICEP2 telescope observed from the South Pole with a 26 cm aperture and cold, on-axis, refractive optics. BICEP2 also adopted a new detector design in which beam-defining slot antenna arrays couple to transition-edge sensor (TES) bolometers, all fabricated on a common substrate. The antenna-coupled TES detectors supported scalable fabrication and multiplexed readout that allowed BICEP2 to achieve a high detector count of 500 bolometers at 150 GHz, giving unprecedented sensitivity to B-modes at degree angular scales. After optimization of detector and readout parameters, BICEP2 achieved an instrument noise-equivalent temperature of 15.8 mu K root s. The full data set reached Stokes Q and U map depths of 87.2 nK in square-degree pixels (5'.2 mu K) over an effective area of 384 deg(2) within a 1000 deg(2) field. These are the deepest CMB polarization maps at degree angular scales to date. The power spectrum analysis presented in a companion paper has resulted in a significant detection of B-mode polarization at degree scales.
C1 [Ade, P. A. R.; Sudiwala, R. V.] Cardiff Univ, Sch Phys & Astron, Cardiff CF24 3AA, S Glam, Wales.
[Aikin, R. W.; Bock, J. J.; Brevik, J. A.; Filippini, J. P.; Golwala, S. R.; Hildebrandt, S. R.; Lueker, M.; Staniszewski, Z. K.; Teply, G. P.] CALTECH, Dept Phys, Pasadena, CA 91125 USA.
[Amiri, M.; Hasselfield, M.] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V5Z 1M9, Canada.
[Barkats, D.] ESO, Joint ALMA Observ, Santiago, Chile.
[Benton, S. J.; Netterfield, C. B.] Univ Toronto, Dept Phys, Toronto, ON, Canada.
[Bischoff, C. A.; Buder, I.; Karkare, K. S.; Kovac, J. M.; Richter, S.; Vieregg, A. G.; Wong, C. L.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Bock, J. J.; Day, P. K.; Dowell, C. D.; Hildebrandt, S. R.; Llombart, N.; Nguyen, H. T.; O'Brient, R.; Turner, A. D.; Wilson, P.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Bullock, E.] Univ Minnesota, Minnesota Inst Astrophys, Minneapolis, MN 55455 USA.
[Duband, L.] Univ Grenoble Alpes, CEA INAC SBT, F-38000 Grenoble, France.
[Fliescher, S.; Schwarz, R.; Sheehy, C. D.] Univ Minnesota, Dept Phys, Minneapolis, MN 55455 USA.
[Hilton, G. C.; Irwin, K. D.; Reintsema, C. D.] NIST, Boulder, CO 80305 USA.
[Irwin, K. D.; Kernasovskiy, S. A.; Kuo, C. L.; Ogburn, R. W.; Tolan, J. E.; Yoon, K. W.] Stanford Univ, Dept Phys, Stanford, CA 94305 USA.
[Irwin, K. D.; Ogburn, R. W.; Yoon, K. W.] Kavli Inst Particle Astrophys & Cosmol, SLAC Natl Accelerator Lab, Menlo Pk, CA 94025 USA.
[Keating, B. G.; Orlando, A.] Univ Calif San Diego, Dept Phys, La Jolla, CA 92093 USA.
[Leitch, E. M.; Sheehy, C. D.; Vieregg, A. G.] Univ Chicago, Chicago, IL 60637 USA.
RP Ade, PAR (reprint author), Cardiff Univ, Sch Phys & Astron, Cardiff CF24 3AA, S Glam, Wales.
EM ogburn@stanford.edu
OI Orlando, Angiola/0000-0001-8004-5054; Karkare,
Kirit/0000-0002-5215-6993; Barkats, Denis/0000-0002-8971-1954; Bischoff,
Colin/0000-0001-9185-6514
FU U.S. National Science Foundation [ANT-0742818, ANT-1044978, ANT-0742592,
ANT-1110087]; NASA APRA and SAT programs [06-ARPA206-0040,
10-SAT10-0017]; Gordon and Betty Moore Foundation at Caltech; Canada
Foundation for Innovation; W.M. Keck Foundation; FAS Science Division
Research Computing Group at Harvard University; JPL Research and
Technology Development Fund
FX BICEP2 was supported by the U.S. National Science Foundation under
grants ANT-0742818 and ANT-1044978 (Caltech/Harvard) and ANT-0742592 and
ANT-1110087 (Chicago/Minnesota). The development of antenna-coupled
detector technology was supported by the JPL Research and Technology
Development Fund and grants 06-ARPA206-0040 and 10-SAT10-0017 from the
NASA APRA and SAT programs. The development and testing of focal planes
were supported by the Gordon and Betty Moore Foundation at Caltech.
Readout electronics were supported by a Canada Foundation for Innovation
grant to UBC. The receiver development was supported in part by a grant
from the W.M. Keck Foundation. The computations in this paper were run
on the Odyssey cluster supported by the FAS Science Division Research
Computing Group at Harvard University. Tireless administrative support
was provided by Irene Coyle and Kathy Deniston.
NR 71
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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 SEP 1
PY 2014
VL 792
IS 1
AR 62
DI 10.1088/0004-637X/792/1/62
PG 29
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AO2RE
UT WOS:000341172100062
ER
PT J
AU Bradley, LD
Zitrin, A
Coe, D
Bouwens, R
Postman, M
Balestra, I
Grillo, C
Monna, A
Rosati, P
Seitz, S
Host, O
Lemze, D
Moustakas, J
Moustakas, LA
Shu, X
Zheng, W
Broadhurst, T
Carrasco, M
Jouvel, S
Koekemoer, A
Medezinski, E
Meneghetti, M
Nonino, M
Smit, R
Umetsu, K
Bartelmann, M
Benitez, N
Donahue, M
Ford, H
Infante, L
Jimenez-Teja, Y
Kelson, D
Lahav, O
Maoz, D
Melchior, P
Merten, J
Molino, A
AF Bradley, L. D.
Zitrin, A.
Coe, D.
Bouwens, R.
Postman, M.
Balestra, I.
Grillo, C.
Monna, A.
Rosati, P.
Seitz, S.
Host, O.
Lemze, D.
Moustakas, J.
Moustakas, L. A.
Shu, X.
Zheng, W.
Broadhurst, T.
Carrasco, M.
Jouvel, S.
Koekemoer, A.
Medezinski, E.
Meneghetti, M.
Nonino, M.
Smit, R.
Umetsu, K.
Bartelmann, M.
Benitez, N.
Donahue, M.
Ford, H.
Infante, L.
Jimenez-Teja, Y.
Kelson, D.
Lahav, O.
Maoz, D.
Melchior, P.
Merten, J.
Molino, A.
TI CLASH: A CENSUS OF MAGNIFIED STAR-FORMING GALAXIES AT z similar to 6-8
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: evolution; galaxies: high-redshift; gravitational lensing:
strong
ID ULTRA-DEEP-FIELD; HIGH-REDSHIFT GALAXIES; LYMAN-BREAK GALAXIES;
EXTRAGALACTIC LEGACY SURVEY; EARLY RELEASE SCIENCE; SPECTRAL
ENERGY-DISTRIBUTIONS; CLUSTER RXC J2248.7-4431; STRONG-LENSING ANALYSIS;
EMISSION-LINE GALAXIES; LUMINOSITY FUNCTION
AB We utilize 16 band Hubble Space Telescope (HST) observations of 18 lensing clusters obtained as part of the Cluster Lensing And Supernova survey with Hubble (CLASH) Multi-Cycle Treasury program to search for z similar to 6-8 galaxies. We report the discovery of 204, 45, and 13 Lyman-break galaxy candidates at z similar to 6, z similar to 7, and z similar to 8, respectively, identified from purely photometric redshift selections. This large sample, representing nearly an order of magnitude increase in the number of magnified star-forming galaxies at z similar to 6-8 presented to date, is unique in that we have observations in four WFC3/UVIS UV, seven ACS/WFC optical, and all five WFC3/IR broadband filters, which enable very accurate photometric redshift selections. We construct detailed lensing models for 17 of the 18 clusters to estimate object magnifications and to identify two new multiply lensed z greater than or similar to 6 candidates. The median magnifications over the 17 clusters are 4, 4, and 5 for the z similar to 6, z similar to 7, and z similar to 8 samples, respectively, over an average area of 4.5 arcmin(2) per cluster. We compare our observed number counts with expectations based on convolving "blank" field UV luminosity functions through our cluster lens models and find rough agreement down to similar to 27 mag, where we begin to suffer significant incompleteness. In all three redshift bins, we find a higher number density at brighter observed magnitudes than the field predictions, empirically demonstrating for the first time the enhanced efficiency of lensing clusters over field surveys. Our number counts also are in general agreement with the lensed expectations from the cluster models, especially at z 6, where we have the best statistics.
C1 [Bradley, L. D.; Coe, D.; Postman, M.; Koekemoer, A.] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
[Zitrin, A.; Carrasco, M.; Bartelmann, M.] Inst Theoret Astrophys, Zentrum Astron, D-29120 Heidelberg, Germany.
[Bouwens, R.; Smit, R.] Leiden Univ, Leiden Observ, Leiden, Netherlands.
[Balestra, I.; Nonino, M.] Osserv Astron Trieste, INAF, I-34143 Trieste, Italy.
[Balestra, I.] Osserv Astron Capodimonte, INAF, I-80131 Naples, Italy.
[Grillo, C.; Host, O.] Univ Copenhagen, Niels Bohr Inst, Dark Cosmol Ctr, DK-2100 Copenhagen, Denmark.
[Monna, A.; Seitz, S.] Univ Observ Munich, D-81679 Munich, Germany.
[Monna, A.; Seitz, S.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany.
[Rosati, P.] European So Observ, D-85748 Garching, Germany.
[Lemze, D.; Zheng, W.; Medezinski, E.; Ford, H.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA.
[Moustakas, J.] Siena Coll, Dept Phys & Astron, Loudonville, NY 12211 USA.
[Moustakas, L. A.; Meneghetti, M.; Merten, J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Shu, X.] Univ Sci & Technol China, Dept Astron, Hefei 230026, Anhui, Peoples R China.
[Broadhurst, T.] Univ Basque Country, UPV EHU, Dept Theoret Phys & Hist Sci, E-48080 Bilbao, Spain.
[Broadhurst, T.] Ikerbasque, Basque Fdn Sci, E-48011 Bilbao, Spain.
[Carrasco, M.] Pontificia Univ Catolica Chile, Ctr Astroingn, Dept Astron & Astrofis, Santiago, Chile.
[Jouvel, S.] CSIC, IEEC, Inst Ciencies Espai, E-08193 Barcelona, Spain.
[Jouvel, S.; Lahav, O.] UCL, Dept Phys & Astron, London WC1E 6BT, England.
[Meneghetti, M.] Osservatorio Astron Bologna, INAF, I-40127 Bologna, Italy.
[Meneghetti, M.] Ist Nazl Fis Nucl, Sez Bologna, I-40127 Bologna, Italy.
[Umetsu, K.] Acad Sinica, Inst Astron & Astrophys, Taipei 10617, Taiwan.
[Benitez, N.; Jimenez-Teja, Y.; Molino, A.] CSIC, IAA, E-18008 Granada, Spain.
[Donahue, M.] Michigan State Univ, Dept Phys & Astron, E Lansing, MI 48824 USA.
[Kelson, D.] Observ Carnegie Inst Washington, Pasadena, CA 91101 USA.
[Maoz, D.] Tel Aviv Univ, Sch Phys & Astron, IL-69978 Tel Aviv, Israel.
[Melchior, P.] Ohio State Univ, Ctr Cosmol & Astro Particle Phys, Columbus, OH 43210 USA.
[Melchior, P.] Ohio State Univ, Dept Phys, Columbus, OH 43210 USA.
RP Bradley, LD (reprint author), Space Telescope Sci Inst, 3700 San Martin Dr, Baltimore, MD 21218 USA.
RI Jimenez-Teja, Yolanda/D-5933-2011; Grillo, Claudio/E-6223-2015;
Meneghetti, Massimo/O-8139-2015; Shu, Xinwen/D-7294-2017;
OI Grillo, Claudio/0000-0002-5926-7143; Meneghetti,
Massimo/0000-0003-1225-7084; Shu, Xinwen/0000-0002-7020-4290; Nonino,
Mario/0000-0001-6342-9662; Balestra, Italo/0000-0001-9660-894X; Umetsu,
Keiichi/0000-0002-7196-4822; Moustakas, Leonidas/0000-0003-3030-2360;
Koekemoer, Anton/0000-0002-6610-2048; Benitez,
Narciso/0000-0002-0403-7455
FU contract research "Internationale Spitzenforschung II/2-6" of the Baden
Wurttemberg Stiftung; DNRF
FX The CLASH Multi-Cycle Treasury Program (GO-12065) is based on
observations made with the NASA/ESA Hubble Space Telescope. The Space
Telescope Science Institute is operatedby the Association of
Universities for Research in Astronomy, Inc. under NASA contract NAS
5-26555. A.Z. is supported by contract research "Internationale
Spitzenforschung II/2-6" of the Baden Wurttemberg Stiftung. The work of
L.A.M., J.M., and M.M. was carried out at the Jet Propulsion Laboratory,
California Institute of Technology, under a contract with NASA. The Dark
Cosmology Centre is funded by the DNRF.
NR 104
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U1 2
U2 17
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 SEP 1
PY 2014
VL 792
IS 1
AR 76
DI 10.1088/0004-637X/792/1/76
PG 19
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AO2RE
UT WOS:000341172100076
ER
PT J
AU Burke, CJ
McCullough, PR
AF Burke, Christopher J.
McCullough, P. R.
TI TRANSIT AND RADIAL VELOCITY SURVEY EFFICIENCY COMPARISON FOR A HABITABLE
ZONE EARTH
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE eclipses; methods: statistical; planetary systems; surveys; techniques:
photometric; techniques: radial velocities
ID SUN-LIKE STAR; MAIN-SEQUENCE STARS; EXTRASOLAR PLANETS; ORBITAL
ECCENTRICITY; FALSE POSITIVES; SPACE-TELESCOPE; BLEND SCENARIOS;
MULTIPLE SYSTEM; LIGHT CURVES; LOW-MASS
AB Transit and radial velocity searches are two techniques for identifying nearby extrasolar planets to Earth that transit bright stars. Identifying a robust sample of these exoplanets around bright stars for detailed atmospheric characterization is a major observational undertaking. In this study we describe a framework that answers the question of whether a transit or radial velocity survey is more efficient at finding transiting exoplanets given the same amount of observing time. Within the framework we show that a transit survey's window function can be approximated using the hypergeometric probability distribution. We estimate the observing time required for a transit survey to find a transiting Earth-sized exoplanet in the habitable zone (HZ) with an emphasis on late-type stars. We also estimate the radial velocity precision necessary to detect the equivalent HZ Earth-mass exoplanet that also transits when using an equal amount of observing time as the transit survey. We find that a radial velocity survey with sigma(rv) similar to 0.6 m s(-1) precision has comparable efficiency in terms of observing time to a transit survey with the requisite photometric precision sigma(phot) similar to 300 ppm to find a transiting Earth-sized exoplanet in the HZ of late M dwarfs. For super-Earths, a sigma(rv) similar to 2.0 m s(-1) precision radial velocity survey has comparable efficiency to a transit survey with sigma(phot) similar to 2300 ppm.
C1 [Burke, Christopher J.] NASA, Ames Res Ctr, SETI Inst, Moffett Field, CA 94035 USA.
[McCullough, P. R.] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
[McCullough, P. R.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA.
RP Burke, CJ (reprint author), NASA, Ames Res Ctr, SETI Inst, Moffett Field, CA 94035 USA.
EM christopher.j.burke@nasa.gov
NR 72
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U1 0
U2 8
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 SEP 1
PY 2014
VL 792
IS 1
AR 79
DI 10.1088/0004-637X/792/1/79
PG 11
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AO2RE
UT WOS:000341172100079
ER
PT J
AU Burke-Spolaor, S
Bannister, KW
AF Burke-Spolaor, Sarah
Bannister, Keith W.
TI THE GALACTIC POSITION DEPENDENCE OF FAST RADIO BURSTS AND THE DISCOVERY
OF FRB011025
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE pulsars: general; radio continuum: general
ID MULTIBEAM PULSAR SURVEY; TRANSIENTS; LATITUDES; SEARCHES; ORIGIN
AB We report the detection of a dispersed fast radio burst (FRB) in archival intermediate-latitude Parkes Radio Telescope data. The burst appears to be of the same physical origin as the four purported extragalactic FRBs reported by Thornton et al. This burst's arrival time precedes the Thornton et al. bursts by 10 years. We consider that this survey, and many other archival low-latitude (vertical bar gb vertical bar < 30 degrees) pulsar surveys, have been searched for FRBs but produced fewer detections than the comparatively brief Thornton et al. search. Such a rate dependence on Galactic position could provide critical supporting evidence for an extragalactic origin for FRBs. To test this, we form an analytic expression to account for Galactic position and survey setup in FRB rate predictions. Employing a sky temperature, scattering, and dispersion model of the Milky Way, we compute the expected number of FRBs if they are isotropically distributed on the sky with respect to the Galactic position (i.e., local), and if they are of extragalactic origin. We demonstrate that the relative detection rates reject a local origin with a confidence of 99.96% (similar to 3.6 sigma). The extragalactic predictions provide a better agreement; however, there are still strong discrepancies with the low-latitude detection rate at a confidence of 99.69% (similar to 2.9 sigma). However, for the extragalactic population, the differences in predicted versus detected population may be accounted for by a number of factors, which we discuss.
C1 [Burke-Spolaor, Sarah] CALTECH, Pasadena, CA 91125 USA.
[Burke-Spolaor, Sarah] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Bannister, Keith W.] CSIRO Astron & Space Sci, Epping, NSW 1710, Australia.
RP Burke-Spolaor, S (reprint author), CALTECH, 1200 East Calif Blvd, Pasadena, CA 91125 USA.
EM sarahbspolaor@gmail.com
OI Bannister, Keith/0000-0003-2149-0363
FU Commonwealth of Australia
FX The Australia Telescope Compact Array Parkes Radio Telescope is part of
the Australia Telescope National Facility, which is funded by the
Commonwealth of Australia for operation as a National Facility managed
by CSIRO. Processing for our archival search was performed on the
Swinburne University Green Machine; we acknowledge the use of this
supercomputer facility in this work. We thank B. Stappers, D. Thornton,
J. Deneva, and A. Brazier for providing information about survey
pointing directions which were used in this paper's analysis. We thank
an anonymous referee for contributing valuable comments on this paper.
Cosmological redshift calculations used the online calculator provided
by Wright (2006).
NR 31
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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 SEP 1
PY 2014
VL 792
IS 1
AR 19
DI 10.1088/0004-637X/792/1/19
PG 7
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AO2RE
UT WOS:000341172100019
ER
PT J
AU Emslie, AG
Holman, GD
Litvinenko, YE
AF Emslie, A. Gordon
Holman, Gordon D.
Litvinenko, Yuri E.
TI ON THE SOLUTION OF THE CONTINUITY EQUATION FOR PRECIPITATING ELECTRONS
IN SOLAR FLARES
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE methods: analytical; plasmas; Sun: atmosphere; Sun: flares; Sun:
particle emission; Sun: X-rays, gamma rays
ID X-RAY OBSERVATIONS; IMPULSIVE PHASE; BREMSSTRAHLUNG; SPECTRA; TARGET;
BEAMS; COLLISIONS
AB Electrons accelerated in solar flares are injected into the surrounding plasma, where they are subjected to the influence of collisional (Coulomb) energy losses. Their evolution is modeled by a partial differential equation describing continuity of electron number. In a recent paper, Dobranskis & Zharkova claim to have found an "updated exact analytical solution" to this continuity equation. Their solution contains an additional term that drives an exponential decrease in electron density with depth, leading them to assert that the well-known solution derived by Brown, Syrovatskii & Shmeleva, and many others is invalid. We show that the solution of Dobranskis & Zharkova results from a fundamental error in the application of the method of characteristics and is hence incorrect. Further, their comparison of the "new" analytical solution with numerical solutions of the Fokker-Planck equation fails to lend support to their result. We conclude that Dobranskis & Zharkova's solution of the universally accepted and well-established continuity equation is incorrect, and that their criticism of the correct solution is unfounded. We also demonstrate the formal equivalence of the approaches of Syrovatskii & Shmeleva and Brown, with particular reference to the evolution of the electron flux and number density (both differential in energy) in a collisional thick target. We strongly urge use of these long-established, correct solutions in future works.
C1 [Emslie, A. Gordon] Western Kentucky Univ, Dept Phys & Astron, Bowling Green, KY 42101 USA.
[Holman, Gordon D.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Litvinenko, Yuri E.] Univ Waikato, Dept Math, Hamilton, New Zealand.
RP Emslie, AG (reprint author), Western Kentucky Univ, Dept Phys & Astron, Bowling Green, KY 42101 USA.
EM emslieg@wku.edu; gordon.d.holman@nasa.gov
FU NASA [NNX10AT78J]; NASA Heliophysics Guest Investigator and Living with
a Star TRT Grants; RHESSI project
FX Useful discussions with Professor Ian Craig are gratefully acknowledged.
A.G.E. was supported by NASA Grant NNX10AT78J. G.D.H. was supported by
NASA Heliophysics Guest Investigator and Living with a Star TR&T Grants
and the RHESSI project. We thank the referee for suggesting the
inclusion of the material in Section 2.2 and the editor for suggesting
that two independently submitted papers with similar content be combined
into the current work.
NR 16
TC 1
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U1 0
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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 SEP 1
PY 2014
VL 792
IS 1
AR 5
DI 10.1088/0004-637X/792/1/5
PG 4
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AO2RE
UT WOS:000341172100005
ER
PT J
AU Hemphill, PB
Rothschild, RE
Markowitz, A
Furst, F
Pottschmidt, K
Wilms, J
AF Hemphill, Paul B.
Rothschild, Richard E.
Markowitz, Alex
Fuerst, Felix
Pottschmidt, Katja
Wilms, Joern
TI A CLUMPY STELLAR WIND AND LUMINOSITY-DEPENDENT CYCLOTRON LINE REVEALED
BY THE FIRST SUZAKU OBSERVATION OF THE HIGH-MASS X-RAY BINARY 4U
1538-522
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE pulsars: individual (4U 1538-522); stars: magnetic field; stars:
oscillations; X-rays: binaries; X-rays: stars
ID OPTICAL SPECTROSCOPY; PULSAR 4U-1538-52; VELA X-1; SPECTRA;
ASTROPHYSICS; ABSORPTION; EVOLUTION; DISCOVERY; BEPPOSAX; MODELS
AB We present results from the first Suzaku observation of the high-mass X-ray binary 4U 1538-522. The broadband spectral coverage of Suzaku allows for a detailed spectral analysis, characterizing the cyclotron resonance scattering feature at 23.0 +/- 0.4 keV and the iron K alpha line at 6.426 +/- 0.008 keV, as well as placing limits on the strengths of the iron K beta line and the iron K edge. We track the evolution of the spectral parameters both in time and in luminosity, notably finding a significant positive correlation between cyclotron line energy and luminosity. A dip and spike in the light curve is shown to be associated with an order-of-magnitude increase in column density along the line of sight, as well as significant variation in the underlying continuum, implying the accretion of a overdense region of a clumpy stellar wind. We also present a phase-resolved analysis, with most spectral parameters of interest showing significant variation with phase. Notably, both the cyclotron line energy and the iron K alpha line intensity vary significantly with phase, with the iron line intensity significantly out of phase with the pulse profile. We discuss the implications of these findings in the context of recent work in the areas of accretion column physics and cyclotron resonance scattering feature formation.
C1 [Hemphill, Paul B.; Rothschild, Richard E.; Markowitz, Alex] Univ Calif San Diego, Ctr Astrophys & Space Sci, La Jolla, CA 92093 USA.
[Markowitz, Alex; Wilms, Joern] Dr Karl Remeis Sternwarte Erlangen Ctr Astroparti, D-96049 Bamberg, Germany.
[Fuerst, Felix] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA.
[Pottschmidt, Katja] Univ Maryland Baltimore Cty, Ctr Space Sci & Technol, Baltimore, MD 21250 USA.
[Pottschmidt, Katja] CRESST, Astrophys Sci Div, Greenbelt, MD 20771 USA.
[Pottschmidt, Katja] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Hemphill, PB (reprint author), Univ Calif San Diego, Ctr Astrophys & Space Sci, 9500 Gilman Dr, La Jolla, CA 92093 USA.
EM pbhemphill@physics.ucsd.edu
RI Wilms, Joern/C-8116-2013; XRAY, SUZAKU/A-1808-2009;
OI Wilms, Joern/0000-0003-2065-5410; Hemphill, Paul/0000-0002-1676-6954
FU NASA [NNX13AE68G]
FX This research has made use of data and software obtained from NASA's
High Energy Astrophysics Science Archive Research Center (HEASARC), a
service of the Goddard Space Flight Center and the Smithsonian
Astrophysical Observatory. P.B.H. was supported by NASA grant
NNX13AE68G.
NR 45
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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 SEP 1
PY 2014
VL 792
IS 1
AR 14
DI 10.1088/0004-637X/792/1/14
PG 15
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AO2RE
UT WOS:000341172100014
ER
PT J
AU Mainzer, A
Bauer, J
Cutri, RM
Grav, T
Masiero, J
Beck, R
Clarkson, P
Conrow, T
Dailey, J
Eisenhardt, P
Fabinsky, B
Fajardo-Acosta, S
Fowler, J
Gelino, C
Grillmair, C
Heinrichsen, I
Kendall, M
Kirkpatrick, JD
Liu, F
Masci, F
McCallon, H
Nugent, CR
Papin, M
Rice, E
Royer, D
Ryan, T
Sevilla, P
Sonnett, S
Stevenson, R
Thompson, DB
Wheelock, S
Wiemer, D
Wittman, M
Wright, E
Yan, L
AF Mainzer, A.
Bauer, J.
Cutri, R. M.
Grav, T.
Masiero, J.
Beck, R.
Clarkson, P.
Conrow, T.
Dailey, J.
Eisenhardt, P.
Fabinsky, B.
Fajardo-Acosta, S.
Fowler, J.
Gelino, C.
Grillmair, C.
Heinrichsen, I.
Kendall, M.
Kirkpatrick, J. Davy
Liu, F.
Masci, F.
McCallon, H.
Nugent, C. R.
Papin, M.
Rice, E.
Royer, D.
Ryan, T.
Sevilla, P.
Sonnett, S.
Stevenson, R.
Thompson, D. B.
Wheelock, S.
Wiemer, D.
Wittman, M.
Wright, E.
Yan, L.
TI INITIAL PERFORMANCE OF THE NEOWISE REACTIVATION MISSION
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE comets: general; infrared: general; minor planets, asteroids: general;
space vehicles; surveys
ID NEAR-EARTH OBJECTS; THERMAL-MODEL CALIBRATION; INFRARED-SURVEY-EXPLORER;
MAIN BELT ASTEROIDS; WISE/NEOWISE OBSERVATIONS; SOLAR-SYSTEM;
POPULATION; METEORITES; DUST; ALBEDO
AB NASA's Wide-field Infrared Survey Explorer (WISE) spacecraft has been brought out of hibernation and has resumed surveying the sky at 3.4 and 4.6 mu m. The scientific objectives of the NEOWISE reactivation mission are to detect, track, and characterize near-Earth asteroids and comets. The search for minor planets resumed on 2013 December 23, and the first new near-Earth object (NEO) was discovered 6 days later. As an infrared survey, NEOWISE detects asteroids based on their thermal emission and is equally sensitive to high and low albedo objects; consequently, NEOWISE-discovered NEOs tend to be large and dark. Over the course of its three-year mission, NEOWISE will determine radiometrically derived diameters and albedos for similar to 2000 NEOs and tens of thousands of Main Belt asteroids. The 32 months of hibernation have had no significant effect on the mission's performance. Image quality, sensitivity, photometric and astrometric accuracy, completeness, and the rate of minor planet detections are all essentially unchanged from the prime mission's post-cryogenic phase.
C1 [Mainzer, A.; Bauer, J.; Masiero, J.; Eisenhardt, P.; Fabinsky, B.; Heinrichsen, I.; Liu, F.; Nugent, C. R.; Rice, E.; Royer, D.; Sonnett, S.; Stevenson, R.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Bauer, J.; Cutri, R. M.; Beck, R.; Conrow, T.; Dailey, J.; Fajardo-Acosta, S.; Fowler, J.; Gelino, C.; Grillmair, C.; Kirkpatrick, J. Davy; Masci, F.; McCallon, H.; Papin, M.; Wheelock, S.; Wittman, M.; Yan, L.] CALTECH, Ctr Infrared Proc & Anal, Pasadena, CA 91125 USA.
[Grav, T.] Planetary Sci Inst, Tucson, AZ USA.
[Clarkson, P.; Kendall, M.; Ryan, T.; Wiemer, D.] Ball Aerosp & Technol Ctr, Boulder, CO USA.
[Sevilla, P.; Thompson, D. B.] Utah State Univ, Space Dynam Lab, Logan, UT 84322 USA.
[Wright, E.] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA.
RP Mainzer, A (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM amainzer@jpl.nasa.gov
OI Masiero, Joseph/0000-0003-2638-720X
FU National Aeronautics and Space Administration
FX This publication makes use of data products from NEOWISE, which is a
project of the Jet Propulsion Laboratory/California Institute of
Technology, funded by the National Aeronautics and Space Administration.
This publication makes use of data products from the Wide-field 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. We thank the paper's referee for helpful comments that
greatly improved the manuscript. We gratefully acknowledge the services
specific to NEOWISE contributed by the International Astronomical
Union's Minor Planet Center, operated by the Harvard-Smithsonian Center
for Astrophysics, and the Central Bureau for Astronomical Telegrams,
operated by Harvard University. We also thank the worldwide community of
dedicated amateur and professional astronomers devoted to minor planet
follow-up observations. This research has made use of the NASA/IPAC
Infrared Science Archive, which is operated by the California Institute
of Technology, under contract with the National Aeronautics and Space
Administration.
NR 61
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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 SEP 1
PY 2014
VL 792
IS 1
AR 30
DI 10.1088/0004-637X/792/1/30
PG 14
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AO2RE
UT WOS:000341172100030
ER
PT J
AU McIntosh, SW
Wang, X
Leamon, RJ
Davey, AR
Howe, R
Krista, LD
Malanushenko, AV
Markel, RS
Cirtain, JW
Gurman, JB
Pesnell, WD
Thompson, MJ
AF McIntosh, Scott W.
Wang, Xin
Leamon, Robert J.
Davey, Alisdair R.
Howe, Rachel
Krista, Larisza D.
Malanushenko, Anna V.
Markel, Robert S.
Cirtain, Jonathan W.
Gurman, Joseph B.
Pesnell, William D.
Thompson, Michael J.
TI DECIPHERING SOLAR MAGNETIC ACTIVITY. I. ON THE RELATIONSHIP BETWEEN THE
SUNSPOT CYCLE AND THE EVOLUTION OF SMALL MAGNETIC FEATURES
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE Sun: activity; Sun: atmosphere; Sun: evolution; Sun: general; Sun:
interior; Sun: rotation; sunspots
ID DIFFERENTIAL ROTATION; MERIDIONAL CIRCULATION; DYNAMO SIMULATION; BRIGHT
POINTS; CORONAL HOLE; SUN-SPOTS; FIELD; FLUX; FLOW; OSCILLATIONS
AB Sunspots are a canonical marker of the Sun's internal magnetic field which flips polarity every similar to 22 yr. The principal variation of sunspots, an similar to 11 yr variation, modulates the amount of the magnetic field that pierces the solar surface and drives significant variations in our star's radiative, particulate, and eruptive output over that period. This paper presents observations from the Solar and Heliospheric Observatory and Solar Dynamics Observatory indicating that the 11 yr sunspot variation is intrinsically tied to the spatio-temporal overlap of the activity bands belonging to the 22 yr magnetic activity cycle. Using a systematic analysis of ubiquitous coronal brightpoints and the magnetic scale on which they appear to form, we show that the landmarks of sunspot cycle 23 can be explained by considering the evolution and interaction of the overlapping activity bands of the longer-scale variability.
C1 [McIntosh, Scott W.; Wang, Xin; Markel, Robert S.; Thompson, Michael J.] Natl Ctr Atmospher Res, High Altitude Observ, Boulder, CO 80307 USA.
[Wang, Xin] Peking Univ, Sch Earth & Space Sci, Beijing 100871, Peoples R China.
[Leamon, Robert J.; Malanushenko, Anna V.] Montana State Univ, Dept Phys, Bozeman, MT 59717 USA.
[Davey, Alisdair R.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Howe, Rachel] Univ Birmingham, Sch Phys & Astron, Birmingham B15 2TT, W Midlands, England.
[Krista, Larisza D.] Univ Colorado, Cooperat Inst Res Environm Sci, Boulder, CO 80205 USA.
[Malanushenko, Anna V.] Lockheed Martin Solar & Astrophys Lab, Palo Alto, CA 94304 USA.
[Cirtain, Jonathan W.] Marshall Space Flight Ctr, Huntsville, AL 35812 USA.
[Gurman, Joseph B.; Pesnell, William D.] NASA, Goddard Space Flight Ctr, Solar Phys Lab, Greenbelt, MD 20771 USA.
RP McIntosh, SW (reprint author), Natl Ctr Atmospher Res, High Altitude Observ, POB 3000, Boulder, CO 80307 USA.
EM mscott@ucar.edu
RI Pesnell, William/D-1062-2012;
OI Pesnell, William/0000-0002-8306-2500; McIntosh,
Scott/0000-0002-7369-1776
FU NASA [NNX08AU30G, NNX08AL23G, NNM07AA01C-Hinode, NNG09FA40C-IRIS,
NNG04EA00C]; National Science Foundation
FX The data used in this paper are openly available from the SOHO, SDO, and
the Virtual Solar Observatory (VSO; http://virtualsolar.org) data
archives. S.W.M., R.J.L., A.R.D., and R.S.M. were partly funded by NASA
grants (NNX08AU30G, NNX08AL23G, NNM07AA01C-Hinode, NNG09FA40C-IRIS).
A.V.M. is supported by NASA grant NNG04EA00C (SDO/AIA). SOHO is a
project of international collaboration between ESA and NASA. Sunspot
data are from David Hathaway and the World Data Center SILSO, Royal
Observatory of Belgium, Brussels. S.W.M. is grateful to Matthias Rempel,
Yuhong Fan, Dick Altrock, SaraMartin, Roger Ulrich, Paul Charbonneau,
Mark Miesch, and Eugene Parker for helpful discussions. NCAR is
sponsored by the National Science Foundation.
NR 53
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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 SEP 1
PY 2014
VL 792
IS 1
AR 12
DI 10.1088/0004-637X/792/1/12
PG 19
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AO2RE
UT WOS:000341172100012
ER
PT J
AU Misra, A
Meadows, V
Crisp, D
AF Misra, Amit
Meadows, Victoria
Crisp, Dave
TI THE EFFECTS OF REFRACTION ON TRANSIT TRANSMISSION SPECTROSCOPY:
APPLICATION TO EARTH-LIKE EXOPLANETS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE astrobiology; planets and satellites: atmospheres; radiative transfer
ID GIANT PLANET TRANSITS; EXTRASOLAR PLANET; MU-M; SPACE-TELESCOPE; LUNAR
ECLIPSE; WATER-VAPOR; ATMOSPHERE; ABSORPTION; MODEL; SPECTRUM
AB We quantify the effects of refraction in transit transmission spectroscopy on spectral absorption features and on temporal variations that could be used to obtain altitude-dependent spectra for planets orbiting stars of different stellar types. We validate our model against altitude-dependent transmission spectra of the Earth from ATMOS and against lunar eclipse spectra from Palle et al. We perform detectability studies to show the potential effects of refraction on hypothetical observations of Earth analogs with the James Webb Space Telescope NIRSPEC. Due to refraction, there will be a maximum tangent pressure level that can be probed during transit for each given planet-star system. We show that because of refraction, for an Earth-analog planet orbiting in the habitable zone of a Sun-like star only the top 0.3 bars of the atmosphere can be probed, leading to a decrease in the signal-to-noise ratio (S/N) of absorption features by 60%, while for an Earth-analog planet orbiting in the habitable zone of an M5V star it is possible to probe almost the entire atmosphere with minimal decreases in S/N. We also show that refraction can result in temporal variations in the transit transmission spectrum which may provide a way to obtain altitude-dependent spectra of exoplanet atmospheres. Additionally, the variations prior to ingress and subsequent to egress provide away to probe pressures greater than the maximum tangent pressure that can be probed during transit. Therefore, probing the maximum range of atmospheric altitudes, and in particular the near-surface environment of an Earth-analog exoplanet, will require looking at out-of-transit refracted light in addition to the in-transit spectrum.
C1 [Misra, Amit; Meadows, Victoria] Univ Washington, Dept Astron, Seattle, WA 98195 USA.
[Misra, Amit; Meadows, Victoria; Crisp, Dave] NAI, Virtual Planetary Lab, Seattle, WA USA.
[Misra, Amit; Meadows, Victoria] Univ Washington, Astrobiol Program, Seattle, WA 98195 USA.
[Crisp, Dave] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Misra, A (reprint author), Univ Washington, Dept Astron, Box 351580, Seattle, WA 98195 USA.
EM amit0@astro.washington.edu
FU National Aeronautics and Space Administration through the NASA
Astrobiology Institute under Cooperative Agreement solicitation
[NNH05ZDA001C]; ARCS Seattle chapter; Astrobiology program at the
University of Washington under an NSF IGERT award
FX This work was performed by the NASA Astrobiology Institute's Virtual
Planetary Laboratory, supported by the National Aeronautics and Space
Administration through the NASA Astrobiology Institute under Cooperative
Agreement solicitation NNH05ZDA001C. This work has also been supported
by a generous fellowship from the ARCS Seattle chapter and funding from
the Astrobiology program at the University of Washington under an NSF
IGERT award.
NR 50
TC 15
Z9 15
U1 0
U2 10
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 SEP 1
PY 2014
VL 792
IS 1
AR 61
DI 10.1088/0004-637X/792/1/61
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AO2RE
UT WOS:000341172100061
ER
PT J
AU Pawellek, N
Krivov, AV
Marshall, JP
Montesinos, B
Abraham, P
Moor, A
Bryden, G
Eiroa, C
AF Pawellek, Nicole
Krivov, Alexander V.
Marshall, Jonathan P.
Montesinos, Benjamin
Abraham, Peter
Moor, Attila
Bryden, Geoffrey
Eiroa, Carlos
TI DISK RADII AND GRAIN SIZES IN HERSCHEL-RESOLVED DEBRIS DISKS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE circumstellar matter; infrared: stars; planetary systems; stars:
individual (GJ 581, HD 9672, HD 10647, HD 10939, HD 13161, HD 14055, HD
17848, HD 20320, HD 21997, HD 23484, HD 27290, HD 48682, HD 50571, HD
71155, HD 71722, HD 95086, HD 95418, HD 102647, HD 104860, HD 109085, HD
110411, HD 125162, HD 139006, HD 142091, HD 161868, HD 170773, HD
172167, HD 182681, HD 188228, HD 195627, HD 197481, HD 207129, HD
216956, HD 218396)
ID STARS NSTARS PROJECT; MAIN-SEQUENCE STARS; SOLAR-TYPE STAR; PLANET
FORMATION; NEARBY STARS; KUIPER-BELT; COLLISIONAL EVOLUTION; DUST
DISTRIBUTIONS; SMALL PARTICLES; BETA-PICTORIS
AB The radii of debris disks and the sizes of their dust grains are important tracers of the planetesimal formation mechanisms and physical processes operating in these systems. Here we use a representative sample of 34 debris disks resolved in various Herschel Space Observatory (Herschel is an ESA space observatory with science instruments provided by European-led Principal Investigator consortia and with important participation from NASA) programs to constrain the disk radii and the size distribution of their dust. While we modeled disks with both warm and cold components, and identified warm inner disks around about two-thirds of the stars, we focus our analysis only on the cold outer disks, i.e., Kuiper-belt analogs. We derive the disk radii from the resolved images and find a large dispersion for host stars of any spectral class, but no significant trend with the stellar luminosity. This argues against ice lines as a dominant player in setting the debris disk sizes, since the ice line location varies with the luminosity of the central star. Fixing the disk radii to those inferred from the resolved images, we model the spectral energy distribution to determine the dust temperature and the grain size distribution for each target. While the dust temperature systematically increases toward earlier spectral types, the ratio of the dust temperature to the blackbody temperature at the disk radius decreases with the stellar luminosity. This is explained by a clear trend of typical sizes increasing toward more luminous stars. The typical grain sizes are compared to the radiation pressure blowout limit S-blow that is proportional to the stellar luminosity-to-mass ratio and thus also increases toward earlier spectral classes. The grain sizes in the disks of G- to A-stars are inferred to be several times S-blow at all stellar luminosities, in agreement with collisional models of debris disks. The sizes, measured in the units of S-blow, appear to decrease with the luminosity, which may be suggestive of the disk's stirring level increasing toward earlier-type stars. The dust opacity index beta ranges between zero and two, and the size distribution index q varies between three and five for all the disks in the sample.
C1 [Pawellek, Nicole; Krivov, Alexander V.] Univ Jena, Inst Astrophys, D-07745 Jena, Germany.
[Pawellek, Nicole; Krivov, Alexander V.] Univ Jena, Universitatssternwarte, D-07745 Jena, Germany.
[Marshall, Jonathan P.] Univ New S Wales, Sch Phys, Sydney, NSW 2052, Australia.
[Marshall, Jonathan P.] Univ New S Wales, Australian Ctr Astrobiol, Sydney, NSW 2052, Australia.
[Marshall, Jonathan P.] Univ Autonoma Madrid, Fac Ciencias, Dept Fis Teor, E-28049 Madrid, Spain.
[Montesinos, Benjamin] CSIC, INTA, CAB, Ctr Astrobiol,Dept Astrofis, E-28691 Madrid, Spain.
[Abraham, Peter; Moor, Attila] Hungarian Acad Sci, Res Ctr Astron & Earth Sci, Konkoly Observ, H-1525 Budapest, Hungary.
[Bryden, Geoffrey] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Pawellek, N (reprint author), Univ Jena, Inst Astrophys, Schillergasschen 2-3, D-07745 Jena, Germany.
RI Montesinos, Benjamin/C-3493-2017;
OI Montesinos, Benjamin/0000-0002-7982-2095; Marshall,
Jonathan/0000-0001-6208-1801
FU DFG [Kr 2164/10-1]; Spanish [AYA 2011-26202]; Hungarian Scientific
Research Fund [OTKA K101393]; Momentum grant of the MTA CSFK Lend "ulet
Disk Research Group
FX We thank Amy Bonsor, Grant Kennedy, Torsten Lohne, and Christian Vitense
for stimulating discussions. N.P. is grateful to Steve Ertel for useful
advice on various aspects of the SED fitting with the thermal annealing
algorithm. Insightful and constructive comments of the anonymous referee
greatly helped to improve the paper. N.P. and A.V.K. acknowledge support
by the DFG through grant Kr 2164/10-1. J.P.M., B.M., C.E. are partly
supported by Spanish grant AYA 2011-26202. This work was also partly
supported by the grant OTKA K101393 of the Hungarian Scientific Research
Fund, and the Momentum grant of the MTA CSFK Lendulet Disk Research
Group.
NR 107
TC 25
Z9 25
U1 0
U2 4
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 SEP 1
PY 2014
VL 792
IS 1
AR 65
DI 10.1088/0004-637X/792/1/65
PG 19
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AO2RE
UT WOS:000341172100065
ER
PT J
AU Pullen, AR
Benson, AJ
Moustakas, LA
AF Pullen, Anthony R.
Benson, Andrew J.
Moustakas, Leonidas A.
TI NONLINEAR EVOLUTION OF DARK MATTER SUBHALOS AND APPLICATIONS TO WARM
DARK MATTER
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE cosmology: theory; dark matter; galaxies: formation; galaxies: halos
ID MILKY-WAY SATELLITES; UNIVERSAL DENSITY PROFILE; GALAXY FORMATION;
NUMERICAL SIMULATIONS; MASS SUBSTRUCTURE; DWARF GALAXIES; LOCAL GROUP;
LAMBDA-CDM; TOO BIG; HALOES
AB We describe the methodology to include nonlinear evolution, including tidal effects, in the computation of subhalo distribution properties in both cold (CDM) and warm (WDM) dark matter universes. Using semi-analytic modeling, we include effects from dynamical friction, tidal stripping, and tidal heating, allowing us to dynamically evolve the subhalo distribution. We calibrate our nonlinear evolution scheme to the CDM subhalo mass function in the Aquarius N-body simulation, producing a subhalo mass function within the range of simulations. We find tidal effects to be the dominant mechanism of nonlinear evolution in the subhalo population. Finally, we compute the subhalo mass function for m(chi) = 1.5 keV WDM including the effects of nonlinear evolution, and compare radial number densities and mass density profiles of subhalos in CDM and WDM models. We show that all three signatures differ between the two dark matter models, suggesting that probes of substructure may be able to differentiate between them.
C1 [Pullen, Anthony R.; Moustakas, Leonidas A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Benson, Andrew J.] Carnegie Observ, Pasadena, CA 91101 USA.
RP Pullen, AR (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM anthony.r.pullen@jpl.nasa.gov
RI Pullen, Anthony/I-7007-2015;
OI Pullen, Anthony/0000-0002-2091-8738; Moustakas,
Leonidas/0000-0003-3030-2360
NR 77
TC 4
Z9 4
U1 0
U2 2
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 SEP 1
PY 2014
VL 792
IS 1
AR 24
DI 10.1088/0004-637X/792/1/24
PG 9
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AO2RE
UT WOS:000341172100024
ER
PT J
AU Ruel, J
Bazin, G
Bayliss, M
Brodwin, M
Foley, RJ
Stalder, B
Aird, KA
Armstrong, R
Ashby, MLN
Bautz, M
Benson, BA
Bleem, LE
Bocquet, S
Carlstrom, JE
Chang, CL
Chapman, SC
Cho, HM
Clocchiatti, A
Crawford, TM
Crites, AT
De Haan, T
Desai, S
Dobbs, MA
Dudley, JP
Forman, WR
George, EM
Gladders, MD
Gonzalez, AH
Halverson, NW
Harrington, NL
High, FW
Holder, GP
Holzapfel, WL
Hrubes, JD
Jones, C
Joy, M
Keisler, R
Knox, L
Lee, AT
Leitch, EM
Liu, J
Lueker, M
Luong-Van, D
Mantz, A
Marrone, DP
McDonald, M
McMahon, JJ
Mehl, J
Meyer, SS
Mocanu, L
Mohr, JJ
Montroy, TE
Murray, SS
Natoli, T
Nurgaliev, D
Padin, S
Plagge, T
Pryke, C
Reichardt, CL
Rest, A
Ruhl, JE
Saliwanchik, BR
Saro, A
Sayre, JT
Schaffer, KK
Shaw, L
Shirokoff, E
Song, J
Suhada, R
Spieler, HG
Stanford, SA
Staniszewski, Z
Starsk, AA
Story, K
Stubbs, CW
Van Engelen, A
Vanderlinde, K
Vieira, JD
Vikhlinin, A
Williamson, R
Zahn, O
Zenteno, A
AF Ruel, J.
Bazin, G.
Bayliss, M.
Brodwin, M.
Foley, R. J.
Stalder, B.
Aird, K. A.
Armstrong, R.
Ashby, M. L. N.
Bautz, M.
Benson, B. A.
Bleem, L. E.
Bocquet, S.
Carlstrom, J. E.
Chang, C. L.
Chapman, S. C.
Cho, H. M.
Clocchiatti, A.
Crawford, T. M.
Crites, A. T.
De Haan, T.
Desai, S.
Dobbs, M. A.
Dudley, J. P.
Forman, W. R.
George, E. M.
Gladders, M. D.
Gonzalez, A. H.
Halverson, N. W.
Harrington, N. L.
High, F. W.
Holder, G. P.
Holzapfel, W. L.
Hrubes, J. D.
Jones, C.
Joy, M.
Keisler, R.
Knox, L.
Lee, A. T.
Leitch, E. M.
Liu, J.
Lueker, M.
Luong-Van, D.
Mantz, A.
Marrone, D. P.
McDonald, M.
McMahon, J. J.
Mehl, J.
Meyer, S. S.
Mocanu, L.
Mohr, J. J.
Montroy, T. E.
Murray, S. S.
Natoli, T.
Nurgaliev, D.
Padin, S.
Plagge, T.
Pryke, C.
Reichardt, C. L.
Rest, A.
Ruhl, J. E.
Saliwanchik, B. R.
Saro, A.
Sayre, J. T.
Schaffer, K. K.
Shaw, L.
Shirokoff, E.
Song, J.
Suhada, R.
Spieler, H. G.
Stanford, S. A.
Staniszewski, Z.
Starsk, A. A.
Story, K.
Stubbs, C. W.
Van Engelen, A.
Vanderlinde, K.
Vieira, J. D.
Vikhlinin, A.
Williamson, R.
Zahn, O.
Zenteno, A.
TI OPTICAL SPECTROSCOPY AND VELOCITY DISPERSIONS OF GALAXY CLUSTERS FROM
THE SPT-SZ SURVEY
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE catalogs; galaxies: clusters: general
ID SOUTH-POLE TELESCOPE; BLANCO COSMOLOGY SURVEY; ZELDOVICH EFFECT SURVEY;
720 SQUARE DEGREES; GREATER-THAN 1; SAMPLE; MASS; ANISOTROPY; REDSHIFTS;
CATALOG
AB We present optical spectroscopy of galaxies in clusters detected through the Sunyaev-Zel'dovich (SZ) effect with the South Pole Telescope (SPT). We report our own measurements of 61 spectroscopic cluster redshifts, and 48 velocity dispersions each calculated with more than 15 member galaxies. This catalog also includes 19 dispersions of SPT-observed clusters previously reported in the literature. The majority of the clusters in this paper are SPT-discovered; of these, most have been previously reported in other SPT cluster catalogs, and five are reported here as SPT discoveries for the first time. By performing a resampling analysis of galaxy velocities, we find that unbiased velocity dispersions can be obtained from a relatively small number of member galaxies (less than or similar to 30), but with increased systematic scatter. We use this analysis to determine statistical confidence intervals that include the effect of membership selection. We fit scaling relations between the observed cluster velocity dispersions and mass estimates from SZ and X-ray observables. In both cases, the results are consistent with the scaling relation between velocity dispersion and mass expected from dark-matter simulations. We measure a similar to 30% log-normal scatter in dispersion at fixed mass, and a similar to 10% offset in the normalization of the dispersion-mass relation when compared to the expectation from simulations, which is within the expected level of systematic uncertainty.
C1 [Ruel, J.; Bayliss, M.; Nurgaliev, D.] Harvard Univ, Dept Phys, Cambridge, MA 02138 USA.
[Bazin, G.; Bocquet, S.; Desai, S.; Liu, J.; Mohr, J. J.; Saro, A.; Suhada, R.; Zenteno, A.] Univ Munich, Dept Phys, D-81679 Munich, Germany.
[Bazin, G.; Bocquet, S.; Desai, S.; Liu, J.; Mohr, J. J.; Zenteno, A.] Excellence Cluster Universe, D-85748 Garching, Germany.
[Bayliss, M.; Foley, R. J.; Stalder, B.; Ashby, M. L. N.; Forman, W. R.; Jones, C.; Murray, S. S.; Starsk, A. A.; Stubbs, C. W.; Vikhlinin, A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Brodwin, M.] Univ Missouri, Dept Phys & Astron, Kansas City, MO 64110 USA.
[Foley, R. J.; Vieira, J. D.] Univ Illinois, Dept Astron, Urbana, IL 61801 USA.
[Foley, R. J.] Univ Illinois, Dept Phys, Urbana, IL 61801 USA.
[Aird, K. A.; Hrubes, J. D.; Luong-Van, D.] Univ Chicago, Chicago, IL 60637 USA.
[Armstrong, R.] Univ Penn, Dept Phys & Astron, Philadelphia, PA 19104 USA.
[Bautz, M.; McDonald, M.] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 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.; Keisler, R.; Leitch, E. M.; Mantz, A.; Mehl, J.; Meyer, S. S.; Mocanu, L.; Natoli, T.; 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.; Meyer, S. S.; Schaffer, K. K.] 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.
[Bleem, L. E.; Carlstrom, J. E.; Chang, C. L.] Argonne Natl Lab, Argonne, IL 60439 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.; Padin, S.; Plagge, T.; Williamson, R.] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA.
[Chapman, S. C.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England.
[Cho, H. M.] NIST Quantum Devices Grp, Boulder, CO 80305 USA.
[Clocchiatti, A.] Pontificia Univ Catolica Chile, Inst Astrofis, Santiago, Chile.
[De Haan, T.; Dobbs, M. A.; Dudley, J. P.; Holder, G. P.; Shaw, L.; Van Engelen, A.] McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada.
[George, E. M.; Harrington, N. L.; Holzapfel, W. L.; Lee, A. T.; Lueker, M.; Reichardt, C. L.; Shirokoff, E.; Zahn, O.] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA.
[Gonzalez, A. H.] Univ Florida, Dept Astron, Gainesville, FL 32611 USA.
[Halverson, N. W.] Univ Colorado, Dept Astrophys & Planetary Sci, Boulder, CO 80309 USA.
[Halverson, N. W.] Univ Colorado, Dept Phys, Boulder, CO 80309 USA.
[Joy, M.] NASA, George C Marshall Space Flight Ctr, Dept Space Sci, Huntsville, AL 35812 USA.
[Knox, L.; Stanford, S. A.] Univ Calif Davis, Dept Phys, Davis, CA 95616 USA.
[Lee, A. T.; Spieler, H. G.] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Div Phys, Berkeley, CA 94720 USA.
[Lueker, M.; Shirokoff, E.; Vieira, J. D.] CALTECH, Pasadena, CA 91125 USA.
[Marrone, D. P.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA.
[McMahon, J. J.; Song, J.] Univ Michigan, Dept Phys, Ann Arbor, MI 48109 USA.
[Mohr, J. J.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany.
[Montroy, T. E.; Ruhl, J. E.; Saliwanchik, B. R.; Sayre, J. T.; Staniszewski, Z.] Case Western Reserve Univ, Ctr Educ & Res Cosmol & Astrophys, Dept Phys, Cleveland, OH 44106 USA.
[Pryke, C.] Univ Minnesota, Dept Phys, Minneapolis, MN 55455 USA.
[Rest, A.] Space Telescope Sci Inst, Baltimore, MD 21218 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.
[Stanford, S. A.] Lawrence Livermore Natl Lab, Inst Geophys & Planetary Phys, Livermore, CA 94551 USA.
[Vanderlinde, K.] Univ Toronto, Dunlap Inst Astron & Astrophys, Toronto, ON M5S 3H4, Canada.
[Vanderlinde, K.] Univ Toronto, Dept Astron & Astrophys, Toronto, ON M5S 3H4, Canada.
[Zahn, O.] Univ Calif Berkeley, Berkeley Ctr Cosmol Phys, Dept Phys, Berkeley, CA 94720 USA.
[Zahn, O.] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Berkeley, CA 94720 USA.
RP Ruel, J (reprint author), Harvard Univ, Dept Phys, 17 Oxford St, Cambridge, MA 02138 USA.
EM mbayliss@cfa.harvard.edu
RI Williamson, Ross/H-1734-2015; Holzapfel, William/I-4836-2015; Stubbs,
Christopher/C-2829-2012;
OI Williamson, Ross/0000-0002-6945-2975; Stubbs,
Christopher/0000-0003-0347-1724; Marrone, Daniel/0000-0002-2367-1080;
Aird, Kenneth/0000-0003-1441-9518; Reichardt,
Christian/0000-0003-2226-9169; Forman, William/0000-0002-9478-1682;
Stark, Antony/0000-0002-2718-9996
FU NASA; National Science Foundation [ANT-0638937]; NSF Physics Frontier
Center [PHY-0114422]; Kavli Foundation; Gordon and Betty Moore
Foundation; NSF [AST-1009012, AST-1009649, MRI-0723073]; NASA [12800071,
12800088, 13800883, NAS 8-03060]; National Sciences and Engineering
Research Council of Canada; Canada Research Chairs program; Canadian
Institute for Advanced Research; Cluster of Excellence "Origin and
Structure of the Universe," - Excellence Initiative of the Federal
Government of Germany, EXC project [153]; Clay Fellowship; KICP
Fellowship; Pennsylvania State University [2834-MIT-SAO-4018]; Alfred P.
Sloan Research Fellowship; Smithsonian Institution; Brinson Foundation;
PFB-06 CATA, Chile; Office of Science of the U.S. Department of Energy
[DE-AC02-05CH11231]; Blanco 4 m at Cerro Tololo Interamerican
Observatories [2005B-0043, 2009B-0400, 2010A-0441, 2010B-0598]
FX Optical imaging data from the Blanco 4 m at Cerro Tololo Interamerican
Observatories (programs 2005B-0043, 2009B-0400, 2010A-0441, 2010B-0598)
are included in this work. Additional imaging data were obtained with
the 6.5 m Magellan Telescopes and the Swope telescope, which are located
at the Las Campanas Observatory in Chile. This work is based in part on
observations made with the Spitzer Space Telescope (PIDs 60099, 70053),
which is operated by the Jet Propulsion Laboratory, California Institute
of Technology under a contract with NASA. Support for this work was
provided by NASA through an award issued by JPL/Caltech.; The South Pole
Telescope program is supported by the National Science Foundation
through grant ANT-0638937. Partial support is also provided by the NSF
Physics Frontier Center grant PHY-0114422 to the Kavli Institute of
Cosmological Physics at the University of Chicago, the Kavli Foundation,
and the Gordon and Betty Moore Foundation. Galaxy cluster research at
Harvard is supported by NSF grant AST-1009012. Galaxy cluster research
at SAO is supported in part by NSF grants AST-1009649 and MRI-0723073.
Support for X-ray analysis was provided by NASA through Chandra Award
Nos. 12800071, 12800088, and 13800883 issued by the Chandra X-Ray
Observatory Center, which is operated by the Smithsonian Astrophysical
Observatory for and on behalf of NASA. The McGill group acknowledges
funding from the National Sciences and Engineering Research Council of
Canada, Canada Research Chairs program, and the Canadian Institute for
Advanced Research. X-ray research at the CfA is supported through NASA
Contract NAS 8-03060. The Munich group was supported by The Cluster of
Excellence "Origin and Structure of the Universe," funded by the
Excellence Initiative of the Federal Government of Germany, EXC project
number 153. R.J.F. is supported by a Clay Fellowship. B. A. B is
supported by a KICP Fellowship, M. B. and M. M. acknowledge support from
contract 2834-MIT-SAO-4018 from the Pennsylvania State University to the
Massachusetts Institute of Technology. M. D. acknowledges support from
an Alfred P. Sloan Research Fellowship, W. F. and C.J. acknowledge
support from the Smithsonian Institution. B. S. acknowledges support
from the Brinson Foundation. A. C. received support from PFB-06 CATA,
Chile. This research used resources of the National Energy Research
Scientific Computing Center, which is supported by the Office of Science
of the U.S. Department of Energy under Contract No. DE-AC02-05CH11231.
NR 58
TC 30
Z9 30
U1 1
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 SEP 1
PY 2014
VL 792
IS 1
AR 45
DI 10.1088/0004-637X/792/1/45
PG 17
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AO2RE
UT WOS:000341172100045
ER
PT J
AU Skemer, AJ
Marley, MS
Hinz, PM
Morzinski, KM
Skrutskie, MF
Leisenring, JM
Close, LM
Saumon, D
Bailey, VP
Briguglio, R
Defrere, D
Esposito, S
Follette, KB
Hill, JM
Males, JR
Puglisi, A
Rodigas, TJ
Xompero, M
AF Skemer, Andrew J.
Marley, Mark S.
Hinz, Philip M.
Morzinski, Katie M.
Skrutskie, Michael F.
Leisenring, Jarron M.
Close, Laird M.
Saumon, Didier
Bailey, Vanessa P.
Briguglio, Runa
Defrere, Denis
Esposito, Simone
Follette, Katherine B.
Hill, John M.
Males, Jared R.
Puglisi, Alfio
Rodigas, Timothy J.
Xompero, Marco
TI DIRECTLY IMAGED L-T TRANSITION EXOPLANETS IN THE MID-INFRARED
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE brown dwarfs; infrared: planetary systems; instrumentation: adaptive
optics; planets and satellites: atmospheres; planets and satellites:
gaseous planets; stars: individual (HR 8799 2M1207 b)
ID PLANETARY-MASS COMPANION; NEAR-INFRARED SPECTROSCOPY; YOUNG BROWN DWARF;
ORBITING HR 8799; EDGE-ON DISK; GIANT PLANETS; MU-M; EXTRASOLAR PLANET;
FINDING CAMPAIGN; CARBON-MONOXIDE
AB Gas-giant planets emit a large fraction of their light in the mid-infrared (greater than or similar to 3 mu m), where photometry and spectroscopy are critical to our understanding of the bulk properties of extrasolar planets. Of particular importance are the L- and M-band atmospheric windows (3-5 mu m), which are the longest wavelengths currently accessible to ground-based, high-contrast imagers. We present binocular LBT adaptive optics (AO) images of the HR 8799 planetary system in six narrow-band filters from 3 to 4 mu m, and a Magellan AO image of the 2M1207 planetary system in a broader 3.3 mu m band. These systems encompass the five known exoplanets with luminosities consistent with L -> T transition brown dwarfs. Our results show that the exoplanets are brighter and have shallower spectral slopes than equivalent temperature brown dwarfs in a wavelength range that contains the methane fundamental absorption feature (spanned by the narrow-band filters and encompassed by the broader 3.3 mu m filter). For 2M1207 b, we find that thick clouds and non-equilibrium chemistry caused by vertical mixing can explain the object's appearance. For the HR 8799 planets, we present new models that suggest the atmospheres must have patchy clouds, along with non-equilibrium chemistry. Together, the presence of a heterogeneous surface and vertical mixing presents a picture of dynamic planetary atmospheres in which both horizontal and vertical motions influence the chemical and condensate profiles.
C1 [Skemer, Andrew J.; Hinz, Philip M.; Morzinski, Katie M.; Leisenring, Jarron M.; Close, Laird M.; Bailey, Vanessa P.; Defrere, Denis; Follette, Katherine B.; Males, Jared R.; Rodigas, Timothy J.] Univ Arizona, Dept Astron, Steward Observ, Tucson, AZ 85721 USA.
[Marley, Mark S.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Skrutskie, Michael F.] Univ Virginia, Dept Astron, Charlottesville, VA 22904 USA.
[Leisenring, Jarron M.] ETH, Inst Astron, CH-8093 Zurich, Switzerland.
[Saumon, Didier] Los Alamos Natl Lab, Los Alamos, NM 87545 USA.
[Briguglio, Runa; Esposito, Simone; Puglisi, Alfio; Xompero, Marco] Osserv Astrofis Arcetri, Ist Nazl Astrofis, I-50125 Florence, Italy.
[Hill, John M.] Univ Arizona, Large Binocular Telescope Observ, Tucson, AZ 85721 USA.
[Rodigas, Timothy J.] Carnegie Inst Sci, Dept Terr Magnetism, Washington, DC 20015 USA.
RP Skemer, AJ (reprint author), Univ Arizona, Dept Astron, Steward Observ, 933 North Cherry Ave, Tucson, AZ 85721 USA.
RI Marley, Mark/I-4704-2013;
OI Esposito, Simone/0000-0002-3114-677X; Xompero,
Marco/0000-0002-5565-084X; Marley, Mark/0000-0002-5251-2943; Skemer,
Andrew/0000-0001-6098-3924; Morzinski, Katie/0000-0002-1384-0063;
Bailey, Vanessa/0000-0002-5407-2806
FU NASA Origins of Solar Systems Program [NNX13AJ17G]; NSF Graduate
Research Fellowship Program [DGE-1143953]; National Aeronautics and
Space Administration, Exoplanet Exploration program; National Science
Foundation [AST-0705296]
FX The authors thank Travis Barman for his insightful comments and for
supplying his 2M1207 b model. We also thank the anonymous referee for
excellent suggestions. This work would not have been possible without
the dedication of the LBTI staff, in particular Vidhya Vaitheeswaran,
who programmed LBTI's rapid filter changing capabilities. A.S. was
supported by the NASA Origins of Solar Systems Program, grant
NNX13AJ17G. V.B. is supported by the NSF Graduate Research Fellowship
Program (DGE-1143953). The Large Binocular Telescope Interferometer is
funded by the National Aeronautics and Space Administration as part of
its Exoplanet Exploration program. LMIRCam is funded by the National
Science Foundation through grant NSF AST-0705296.
NR 88
TC 34
Z9 34
U1 0
U2 0
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 SEP 1
PY 2014
VL 792
IS 1
AR 17
DI 10.1088/0004-637X/792/1/17
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AO2RE
UT WOS:000341172100017
ER
PT J
AU Wik, DR
Hornstrup, A
Molendi, S
Madejski, G
Harrison, FA
Zoglauer, A
Grefenstette, BW
Gastaldello, F
Madsen, KK
Westergaard, NJ
Ferreira, DDM
Kitaguchi, T
Pedersen, K
Boggs, SE
Christensen, FE
Craig, WW
Hailey, CJ
Stern, D
Zhang, WW
AF Wik, Daniel R.
Hornstrup, A.
Molendi, S.
Madejski, G.
Harrison, F. A.
Zoglauer, A.
Grefenstette, B. W.
Gastaldello, F.
Madsen, K. K.
Westergaard, N. J.
Ferreira, D. D. M.
Kitaguchi, T.
Pedersen, K.
Boggs, S. E.
Christensen, F. E.
Craig, W. W.
Hailey, C. J.
Stern, D.
Zhang, W. W.
TI NuSTAR OBSERVATIONS OF THE BULLET CLUSTER: CONSTRAINTS ON INVERSE
COMPTON EMISSION
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: clusters: general; galaxies: clusters: individual (Bullet
cluster); intergalactic medium; magnetic fields; radiation mechanisms:
non-thermal; X-rays: galaxies: clusters
ID X-RAY-SPECTRA; HOTTEST KNOWN CLUSTER; GALAXY CLUSTERS; COMA CLUSTER;
MAGNETIC-FIELDS; 1E 0657-56; NONTHERMAL EMISSION; EXCESS EMISSION;
XMM-NEWTON; CHANDRA
AB The search for diffuse non-thermal inverse Compton (IC) emission from galaxy clusters at hard X-ray energies has been undertaken with many instruments, with most detections being either of low significance or controversial. Because all prior telescopes sensitive at E > 10 keV do not focus light and have degree-scale fields of view, their backgrounds are both high and difficult to characterize. The associated uncertainties result in lower sensitivity to IC emission and a greater chance of false detection. In this work, we present 266 ks NuSTAR observations of the Bullet cluster, which is detected in the energy range 3-30 keV. NuSTAR's unprecedented hard X-ray focusing capability largely eliminates confusion between diffuse IC and point sources; however, at the highest energies, the background still dominates and must be well understood. To this end, we have developed a complete background model constructed of physically inspired components constrained by extragalactic survey field observations, the specific parameters of which are derived locally from data in non-source regions of target observations. Applying the background model to the Bullet cluster data, we find that the spectrum is well-but not perfectly-described as an isothermal plasma with kT = 14.2 +/- 0.2 keV. To slightly improve the fit, a second temperature component is added, which appears to account for lower temperature emission from the cool core, pushing the primary component to kT similar to 15.3 keV. We see no convincing need to invoke an IC component to describe the spectrum of the Bullet cluster, and instead argue that it is dominated at all energies by emission from purely thermal gas. The conservatively derived 90% upper limit on the IC flux of 1.1 x 10(-12) erg s(-1) cm(-2) (50-100 keV), implying a lower limit on B greater than or similar to 0.2 mu G, is barely consistent with detected fluxes previously reported. In addition to discussing the possible origin of this discrepancy, we remark on the potential implications of this analysis for the prospects for detecting IC in galaxy clusters in the future.
C1 [Wik, Daniel R.; Zhang, W. W.] NASA, Astrophys Sci Div, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Wik, Daniel R.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA.
[Hornstrup, A.; Westergaard, N. J.; Ferreira, D. D. M.; Pedersen, K.; Christensen, F. E.] Tech Univ Denmark, Natl Space Inst, DTU Space, DK-2800 Lyngby, Denmark.
[Molendi, S.; Gastaldello, F.] INAF, IASF Milano, I-20133 Milan, Italy.
[Madejski, G.] SLAC Natl Accelerator Lab, Kavli Inst Particle Astrophys & Cosmol, Menlo Pk, CA 94025 USA.
[Harrison, F. A.; Grefenstette, B. W.; Madsen, K. K.] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA.
[Zoglauer, A.; Boggs, S. E.; Craig, W. W.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
[Kitaguchi, T.] RIKEN, Nishina Ctr, Wako, Saitama 3510198, Japan.
[Craig, W. W.] Lawrence Livermore Natl Lab, Livermore, CA 94550 USA.
[Hailey, C. J.] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA.
[Stern, D.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Wik, DR (reprint author), NASA, Astrophys Sci Div, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
EM daniel.r.wik@nasa.gov
RI Boggs, Steven/E-4170-2015; Gastaldello, Fabio/N-4226-2015; Ferreira,
Desiree/M-1666-2016;
OI Boggs, Steven/0000-0001-9567-4224; Gastaldello,
Fabio/0000-0002-9112-0184; Ferreira, Desiree/0000-0003-4003-3256;
Molendi, Silvano/0000-0002-2483-278X
NR 43
TC 51
Z9 51
U1 0
U2 2
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 SEP 1
PY 2014
VL 792
IS 1
AR 48
DI 10.1088/0004-637X/792/1/48
PG 24
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AO2RE
UT WOS:000341172100048
ER
PT J
AU Zhai, CX
Shao, M
Nemati, BJ
Werne, T
Zhou, HY
Turyshev, SG
Sandhu, J
Hallinan, G
Harding, LK
AF Zhai, Chengxing
Shao, Michael
Nemati, Bijan
Werne, Thomas
Zhou, Hanying
Turyshev, Slava G.
Sandhu, Jagmit
Hallinan, Gregg
Harding, Leon K.
TI DETECTION OF A FAINT FAST-MOVING NEAR-EARTH ASTEROID USING THE SYNTHETIC
TRACKING TECHNIQUE
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE astrometry; atmospheric effects; methods: data analysis; methods:
observational; minor planets, asteroids: general
ID PHOTOMETRY
AB We report a detection of a faint near-Earth asteroid (NEA) using our synthetic tracking technique and the CHIMERA instrument on the Palomar 200 inch telescope. With an apparent magnitude of 23 (H = 29, assuming detection at 20 lunar distances), the asteroid was moving at 6 degrees.32 day(-1) and was detected at a signal-to-noise ratio (S/N) of 15 using 30 s of data taken at a 16.7 Hz frame rate. The detection was confirmed by a second observation 77 minutes later at the same S/N. Because of its high proper motion, the NEA moved 7 arcsec over the 30 s of observation. Synthetic tracking avoided image degradation due to trailing loss that affects conventional techniques relying on 30 s exposures; the trailing loss would have degraded the surface brightness of the NEA image on the CCD down to an approximate magnitude of 25 making the object undetectable. This detection was a result of our 12 hr blind search conducted on the Palomar 200 inch telescope over two nights, scanning twice over six (5 degrees.3 x 0 degrees.046) fields. Detecting only one asteroid is consistent with Harris's estimates for the distribution of the asteroid population, which was used to predict a detection of 1.2 NEAs in the H-magnitude range 28-31 for the two nights. The experimental design, data analysis methods, and algorithms are presented. We also demonstrate milliarcsecond-level astrometry using observations of two known bright asteroids on the same system with synthetic tracking. We conclude by discussing strategies for scheduling observations to detect and characterize small and fast-moving NEAs using the new technique.
C1 [Zhai, Chengxing; Shao, Michael; Nemati, Bijan; Werne, Thomas; Zhou, Hanying; Turyshev, Slava G.; Sandhu, Jagmit] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Hallinan, Gregg; Harding, Leon K.] CALTECH, Dept Astron, Pasadena, CA 91125 USA.
RP Zhai, CX (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM chengxing.zhai@jpl.nasa.gov
NR 20
TC 8
Z9 8
U1 1
U2 8
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 SEP 1
PY 2014
VL 792
IS 1
AR 60
DI 10.1088/0004-637X/792/1/60
PG 14
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AO2RE
UT WOS:000341172100060
ER
PT J
AU Zwart, SR
Launius, RD
Coen, GK
Morgan, JLL
Charles, JB
Smith, SM
AF Zwart, Sara R.
Launius, Ryan D.
Coen, Geoffrey K.
Morgan, Jennifer L. L.
Charles, John B.
Smith, Scott M.
TI Body Mass Changes During Long-Duration Spaceflight
SO AVIATION SPACE AND ENVIRONMENTAL MEDICINE
LA English
DT Article
DE body mass; energy intake; spaceflight; weightlessness
ID INTERNATIONAL-SPACE-STATION; ENERGY-EXPENDITURE; NUTRITIONAL-STATUS;
FLIGHT; HUMANS; ASTRONAUTS; BONE
AB Background: During early spaceflights, many crewmembers did not meet their caloric requirements and consequently lost body mass during flight, as assessed by a decrease in postflight body mass. Maintaining body mass during spaceflight is crucial for maintaining crew health and monitoring body mass is thus important to medical operations as well as being a key component of human research. Determining body mass becomes difficult in a microgravity environment. Methods: We report data from two mass measurement devices on the International Space Station (ISS): the Russian body mass measuring device (BMMD), which uses spring oscillation physics, and NASA's Space Linear Acceleration Mass Measurement Device (SLAMMD), which uses Newton's second law of motion (F = ma). Results: For 25 crewmembers whose body mass was measured on both devices, significant body mass loss occurred compared to preflight (gravimetric scale) and averaged -4.4% as assessed by BMMD and -2.8% as assessed by SLAMMD. After an initial loss in the first 30 d of flight, body mass remained constant through the rest of the mission, as determined using either device. The mean difference between the two devices was 1.1 kg when the closest SLAMMD and BMMD measurements were compared (6.9 +/- 6.2 d apart). Dietary intake during flight is approximately 80% of the World Health Organization estimated requirement and the decrease in body mass follows in-flight energy intake closely on average. Conclusion: Body mass monitoring is important for monitoring crew health during a mission and to help ensure that crewmembers consume adequate energy intake to mitigate the risks of spaceflight.
C1 [Zwart, Sara R.; Launius, Ryan D.; Coen, Geoffrey K.; Morgan, Jennifer L. L.; Charles, John B.; Smith, Scott M.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA.
RP Smith, SM (reprint author), NASA, Lyndon B Johnson Space Ctr, Mail Code SK3,2101 NASA Pkwy, Houston, TX 77058 USA.
EM scott.m.smith@nasa.gov
FU NASA Human Research Program's Human Health and Countermeasure Element
FX We thank the astronauts who participated in these studies for their time
and effort, and the staff of the NASA Johnson Space Center Nutritional
Biochemistry Laboratory for their efforts in all aspects of carrying out
this project. We thank Jane Krauhs for editorial assistance. This study
was funded by the NASA Human Research Program's Human Health and
Countermeasure Element.
NR 21
TC 6
Z9 6
U1 0
U2 6
PU AEROSPACE MEDICAL ASSOC
PI ALEXANDRIA
PA 320 S HENRY ST, ALEXANDRIA, VA 22314-3579 USA
SN 0095-6562
EI 1943-4448
J9 AVIAT SPACE ENVIR MD
JI Aviat. Space Environ. Med.
PD SEP
PY 2014
VL 85
IS 9
BP 897
EP 904
DI 10.3357/ASEM.3979.2014
PG 8
WC Public, Environmental & Occupational Health; Medicine, General &
Internal; Sport Sciences
SC Public, Environmental & Occupational Health; General & Internal
Medicine; Sport Sciences
GA AN7XD
UT WOS:000340813400001
PM 25197887
ER
PT J
AU Somers, JT
Gohmert, DM
Brinkley, JW
AF Somers, Jeffrey T.
Gohmert, Dustin M.
Brinkley, James W.
TI Spacecraft Occupant Protection Requirements: A Review of the Recent
Changes
SO AVIATION SPACE AND ENVIRONMENTAL MEDICINE
LA English
DT Review
DE injury biomechanics; Hybrid III; multi-axial dynamic response criterion;
Brinkley model; anthropomorphic test device; impact biomechanics
ID CERVICAL-SPINE; HUMAN RESPONSE; STRUCTURAL-PROPERTIES; SPACEFLIGHT;
IMPACTS; INJURY; CONCUSSION; FOOTBALL; MUSCLE; RISK
AB NASA has recently updated spacecraft design requirements for protecting crewmembers during dynamic spaceflight phases. The details of the update are available in a NASA publication (NASA TM-2013-217380) and are summarized here. Previously, NASA's occupant protection requirements relied primarily on the multiaxial dynamic response criterion, which NASA refers to as the Brinkley Dynamic Response Criteria (BDRC). Although simple to implement, there are several important ground rules that must be met for the injury predictions to be applicable. These include proper restraint, flail controls, proper seating support, pressure suit considerations, head protection including consideration of helmet mass, and spaceflight deconditioning. Even if these ground rules are met, there are limitations to the model that must be addressed, including: model validation, sex differences, age effects, anthropometry effects, and differences between the physical fitness of military test subjects and future crewmembers. To address these limitations, new injury assessment reference values (IARV) have been prescribed for the 5th percentile female and 95th percentile male Hybrid III anthropomorphic test devices (ATD). These metrics are head-injury criterion, head-rotational acceleration, neck injury criterion, neck-axial-force limits, flail prevention, and lumbar-axial compression force. Using these new ATD IARVs, NASA can have increased confidence that vehicle designs mitigate the risk of injury during dynamic phases of flight.
C1 NASA Johnson Space Ctr, Wyle Sci Technol & Engn Grp, Houston, TX USA.
NASA Johnson Space Ctr, Crew & Thermal Syst Div, Houston, TX USA.
RP Somers, JT (reprint author), 1290 Hercules Dr, Houston, TX 77058 USA.
EM jeff.somers@nasa.gov
RI Somers, Jeffrey/N-4168-2014
OI Somers, Jeffrey/0000-0003-3347-6614
FU NASA Human Research Program, Johnson Space Center (JSC) Health and Human
Performance Directorate; JSC Engineering Directorate; [NAS9-02078]
FX This work was funded by the NASA Human Research Program, Johnson Space
Center (JSC) Health and Human Performance Directorate, and the JSC
Engineering Directorate. Portions of the work were performed under the
Bioastronautics Contract (NAS9-02078). In addition, the authors would
like especially thank the NASA Engineering and Safety Center and outside
experts for their thorough review of the proposed requirements.
NR 73
TC 1
Z9 1
U1 1
U2 12
PU AEROSPACE MEDICAL ASSOC
PI ALEXANDRIA
PA 320 S HENRY ST, ALEXANDRIA, VA 22314-3579 USA
SN 0095-6562
EI 1943-4448
J9 AVIAT SPACE ENVIR MD
JI Aviat. Space Environ. Med.
PD SEP
PY 2014
VL 85
IS 9
BP 940
EP 948
DI 10.3357/ASEM.4004.2014
PG 9
WC Public, Environmental & Occupational Health; Medicine, General &
Internal; Sport Sciences
SC Public, Environmental & Occupational Health; General & Internal
Medicine; Sport Sciences
GA AN7XD
UT WOS:000340813400007
PM 25197893
ER
PT J
AU Godinez, A
Liston, DB
Ayzenberg, R
Toscano, WB
Cowings, PA
Stone, LS
AF Godinez, Angelica
Liston, Dorion B.
Ayzenberg, Ruthie
Toscano, William B.
Cowings, Patricia A.
Stone, Leland S.
TI G-Loading and Vibration Effects on Heart and Respiration Rates
SO AVIATION SPACE AND ENVIRONMENTAL MEDICINE
LA English
DT Article
DE stress; launch; ascent; interaction; autonomic nervous system
ID SUSTAINED ACCELERATION; MECHANICAL IMPEDANCE; BODY
AB Background: Operational environments expose pilots and astronauts to sustained acceleration (G loading) and whole-body vibration, alone and in combination. Separately, the physiological effects of G loading and vibration have been well studied; both have effects similar to mild exercise. The few studies of combined G loading and vibration have not reported an interaction between these factors on physiological responses. Methods: We tested the effects of G loading (+1 and +3.8 G(x)) and vibration (0.5 g(x) at 8, 12, and 16 Hz), alone and in combination, on heart and respiration rate. Results: We observed an effect of G loading on heart rate (average increase of 23 bpm, SD: 12) and respiration rate (average increase of 5 breaths per minute, SD: 5), an effect of vibration on heart rate, and an interaction on heart rate. With vibration, we observed heart rate increases of 4 bpm (SD: 3) with no increase in respiration rate. In the +1 G(x) condition, the largest heart rate increase occurred during low-frequency (8 Hz) vibration, while at +3.8 G(x), the largest heart rate increase occurred during high-frequency (16 Hz) vibration, demonstrating interaction. Discussion: Consistent with previous reports, our G-loading and vibration effects are similar to mild exercise. In addition, we observed an interaction between G loading and vibration on heart rate, with maximum heart rates occurring at a higher vibration frequency at +3.8 G(x) compared to +1 G(x). The observed interaction demonstrates that G-loading and vibration effects are not independent and can only be properly assessed during combined exposure.
C1 [Godinez, Angelica; Liston, Dorion B.] San Jose State Univ, San Jose, CA 95192 USA.
[Ayzenberg, Ruthie] Santa Clara Univ, Santa Clara, CA 95053 USA.
[Toscano, William B.; Cowings, Patricia A.; Stone, Leland S.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
RP Stone, LS (reprint author), NASA, Ames Res Ctr, Mail Stop 262-2,POB 1, Moffett Field, CA 94035 USA.
EM leland.s.stone@nasa.gov
FU National Space Biomedical Research Institute [SA002002]
FX This work was supported by grant SA002002 from the National Space
Biomedical Research Institute.
NR 15
TC 2
Z9 2
U1 1
U2 3
PU AEROSPACE MEDICAL ASSOC
PI ALEXANDRIA
PA 320 S HENRY ST, ALEXANDRIA, VA 22314-3579 USA
SN 0095-6562
EI 1943-4448
J9 AVIAT SPACE ENVIR MD
JI Aviat. Space Environ. Med.
PD SEP
PY 2014
VL 85
IS 9
BP 949
EP 953
DI 10.3357/ASEM.4015.2014
PG 5
WC Public, Environmental & Occupational Health; Medicine, General &
Internal; Sport Sciences
SC Public, Environmental & Occupational Health; General & Internal
Medicine; Sport Sciences
GA AN7XD
UT WOS:000340813400008
PM 25197894
ER
PT J
AU Gatti, E
Villa, IM
Achyuthan, H
Gibbard, PL
Oppenheimer, C
AF Gatti, E.
Villa, I. M.
Achyuthan, H.
Gibbard, P. L.
Oppenheimer, C.
TI Geochemical variability in distal and proximal glass from the Youngest
Toba Tuff eruption
SO BULLETIN OF VOLCANOLOGY
LA English
DT Article
DE Youngest Toba Tuff; Chemical variability; Crystal fractionation;
Post-depositional alteration; Oldest Toba Tuff
ID SOUTH CHINA SEA; SUPER-ERUPTION; VOLCANIC ASH; 75 KA; INDIAN
SUBCONTINENT; PENINSULAR INDIA; AR-40/AR-39 AGE; NORTH SUMATRA; TEPHRA;
INDONESIA
AB The Youngest Toba Tuff (YTT, erupted at ca. 74 ka) is a distinctive and widespread tephra marker across South and Southeast Asia. The climatic, human and environmental consequences of the YTT eruption are widely debated. Although a considerable body of geochemical data is available for this unit, there has not been a systematic study of the variability of the ash geochemistry. Intrinsic (magmatic) and extrinsic (post-depositional) chemical variations bring fundamental information regarding the petrogenesis of the magma, the distribution of the tephra and the interaction between the ash and the receiving environment. Considering the importance of the geochemistry of the YTT for stratigraphic correlations and eruptive models, it is central to the YTT debate to quantify and interpret such variations. Here, we collate all published geochemical data on the YTT glass, including analyses from 67 sites described in the literature and three new samples. Two principal sources of chemical variation are investigated: (i) compositional zonation of the magma reservoir and (ii) post-depositional alteration. Post-depositional leaching is responsible for up to ca. 11 % differences in Na2O/K2O and ca. 1 % differences in SiO2/Al2O3 ratios in YTT glass from marine sites. Continental tephras are 2 % higher in Na2O/K2O and 3 % higher in SiO2/Al2O3 with respect to the marine tephra. We interpret such post-depositional glass alteration as related to seawater-induced alkali migration in marine environments. Crystal fractionation and consequential magmatic differentiation, which produced order-of-magnitude variations in trace element concentrations reported in the literature, also produced major element differences in the YTT glass. FeO/Al2O3 ratios vary by about 50 %, which is analytically significant. These variations represent magmatic fractionation involving Fe-bearing phases. We also compared major element concentrations in YTT and Oldest Toba Tuff (OTT) ash samples, to identify potential compositional differences that could constrain the stratigraphic identity of the Morgaon ash (western India); no differences between the OTT and YTT samples were observed.
C1 [Gatti, E.; Gibbard, P. L.; Oppenheimer, C.] Univ Cambridge, Dept Geog, Cambridge CB2 3EN, England.
[Villa, I. M.] Univ Bern, Inst Geol, CH-3012 Bern, Switzerland.
[Villa, I. M.] Univ Milano Bicocca, I-20126 Milan, Italy.
[Achyuthan, H.] Anna Univ, Dept Geol, Chennai 600025, Tamil Nadu, India.
RP Gatti, E (reprint author), CALTECH, Jet Prop Lab, NASA, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM emma.gatti@jpl.nasa.gov
RI Oppenheimer, Clive/G-9881-2013
OI Oppenheimer, Clive/0000-0003-4506-7260
FU Dudley Stamp Memorial Award (Royal Geographical Society);
Cambridge-India Partnership; SMUTS Memorial Fund; Philip Lake Fund;
Sidney Sussex College; William George Fearnsides Fund (Geological
Society of London)
FX This work was supported by the Dudley Stamp Memorial Award (Royal
Geographical Society), the Cambridge-India Partnership, the SMUTS
Memorial Fund, Philip Lake Fund, Sidney Sussex College and the William
George Fearnsides Fund (Geological Society of London). We thank Rachna
Raj, Alpa Shridar, L.S. Chamyal, N. Karmalkar and V. Kale for support
provided during fieldwork. E. G. particularly thanks Steve Boreham,
Chris Rolfe, Chiara Petrone and Jason Day for facilitating her work in
the Geography Science Laboratories, Department of Geography and in the
Department of Earth Sciences at the University of Cambridge. We also
thank Sacha Jones for providing ash samples from Jwalapuram and Hermann
Kudrass for providing information about the Bay of Bengal cores. We
thank the editors and the anonymous reviewers of the original manuscript
for their valuable comments.
NR 70
TC 3
Z9 3
U1 7
U2 22
PU SPRINGER
PI NEW YORK
PA 233 SPRING ST, NEW YORK, NY 10013 USA
SN 0258-8900
EI 1432-0819
J9 B VOLCANOL
JI Bull. Volcanol.
PD SEP
PY 2014
VL 76
IS 9
AR 859
DI 10.1007/s00445-014-0859-x
PG 16
WC Geosciences, Multidisciplinary
SC Geology
GA AO5EM
UT WOS:000341366100009
ER
PT J
AU Kitamura, K
Liou, MS
Chang, CH
AF Kitamura, Keiichi
Liou, Meng-Sing
Chang, Chih-Hao
TI Extension and Comparative Study of AUSM-Family Schemes for Compressible
Multiphase Flow Simulations
SO COMMUNICATIONS IN COMPUTATIONAL PHYSICS
LA English
DT Article
DE Multiphase flow; two-fluid model; AUSM-family; stratified flow model
ID HYPERSONIC HEATING COMPUTATIONS; GHOST FLUID METHOD; 2-PHASE FLOW;
NUMERICAL-METHOD; EULER FLUXES; ACCURATE; INTERFACE; EQUATIONS; MODELS;
SEQUEL
AB Several recently developed AUSM-family numerical flux functions (SLAU, SLAU2, AUSM(+)-up2, and AUSMPW+) have been successfully extended to compute compressible multiphase flows, based on the stratified flow model concept, by following two previous works: one by M.-S. Liou, C.-H. Chang, L. Nguyen, and T. G. Theofanous [AIAA J. 46:2345-2356, 2008], in which AUSM(+)-up was used entirely, and the other by C.-H. Chang, and M.-S. Liou [J. Comput. Phys. 225:840-873, 2007], in which the exact Riemann solver was combined into AUSM(+)-up at the phase interface. Through an extensive survey by comparing flux functions, the following are found: (1) AUSM(+)-up with dissipation parameters of K-p and K-u equal to 0.5 or greater, AUSMPW+, SLAU2, AUSM(+)-up2, and SLAU can be used to solve benchmark problems, including a shock/water-droplet interaction; (2) SLAU shows oscillatory behaviors [though not as catastrophic as those of AUSM(+) (a special case of AUSM(+)-up with K-p - K-u - 0)] due to insufficient dissipation arising from its ideal-gas-based dissipation term; and (3) when combined with the exact Riemann solver, AUSM(+)-up (K-p = K-u = 1), SLAU2, and AUSMPW+ are applicable to more challenging problems with high pressure ratios.
C1 [Kitamura, Keiichi; Liou, Meng-Sing] NASA Glenn Res Ctr, Cleveland, OH 44135 USA.
[Kitamura, Keiichi] JAXAs Engn Digital Innovat JEDI Ctr, JSPS, Chuo Ku, Sagamihara, Kanagawa, Japan.
[Kitamura, Keiichi] Nagoya Univ, Chikusa Ku, Nagoya, Aichi 4648603, Japan.
[Chang, Chih-Hao] Theofanous & Co Inc, Santa Barbara, CA 93109 USA.
RP Kitamura, K (reprint author), Yokohama Natl Univ, Hodogaya Ku, Yokohama, Kanagawa 2408501, Japan.
EM kitamura@ynu.ac.jp; meng-sing.liou@nasa.gov; chchang@theofanous.net
RI KITAMURA, Keiichi/M-5488-2014
OI KITAMURA, Keiichi/0000-0001-7550-8990
NR 59
TC 2
Z9 2
U1 0
U2 9
PU GLOBAL SCIENCE PRESS
PI WANCHAI
PA ROOM 3208, CENTRAL PLAZA, 18 HARBOUR RD, WANCHAI, HONG KONG 00000,
PEOPLES R CHINA
SN 1815-2406
EI 1991-7120
J9 COMMUN COMPUT PHYS
JI Commun. Comput. Phys.
PD SEP
PY 2014
VL 16
IS 3
BP 632
EP 674
DI 10.4208/cicp.020813.190214a
PG 43
WC Physics, Mathematical
SC Physics
GA AN7NS
UT WOS:000340787900004
ER
PT J
AU Hurford, TA
Brunt, KM
AF Hurford, T. A.
Brunt, K. M.
TI Antarctic analog for dilational bands on Europa
SO EARTH AND PLANETARY SCIENCE LETTERS
LA English
DT Article
DE Europa; tectonics; Earth analog; Antarctica
ID ROSS ICE SHELF; ENCELADUS; MORPHOLOGY; MODEL; TECTONICS; FRACTURES;
SURFACE; FLEXURE; RIDGES; TIDES
AB Europa's surface shows signs of extension, which is revealed as lithospheric dilation expressed along ridges, dilational bands and ridged bands. Ridges, the most common tectonic feature on Europa, comprise a central crack flanked by two raised banks a few hundred meters high on each side. Together these three classes may represent a continuum of formation. In Tufts' Dilational Model ridge formation is dominated by daily tidal cycling of a crack, which can be superimposed with regional secular dilation. The two sources of dilation can combine to form the various band morphologies observed. New GPS data along a rift on the Ross Ice Shelf, Antarctica is a suitable Earth analog to test the framework of Tufts' Dilational Model. As predicted by Tufts' Dilational Model, tensile failures in the Ross Ice Shelf exhibit secular dilation, upon which a tidal signal can be seen. From this analog we conclude that Tufts' Dilational Model for Europan ridges and bands may be credible and that the secular dilation is most likely from a regional source and not tidally driven. Published by Elsevier B.V.
C1 [Hurford, T. A.] NASA, Planetary Syst Lab, Goddard Spaceflight Ctr, Greenbelt, MD 20771 USA.
[Brunt, K. M.] Univ Maryland, ESSIC, College Pk, MD 20740 USA.
[Brunt, K. M.] NASA, Cryospher Sci Lab, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Hurford, TA (reprint author), NASA, Planetary Syst Lab, Goddard Spaceflight Ctr, Greenbelt, MD 20771 USA.
EM Terry.A.Hurford@nasa.gov
RI Hurford, Terry/F-2625-2012
FU NASA Headquarters
FX We thank NASA Headquarters for funding through the Science Innovation
Fund (Surface Deformation of Icy Moons: Insights from Earth Analogs and
Modeling). We thank Douglas MacAyeal and the NSIDC for Nascent Iceberg
GPS data. We thank Jeanne Sauber, Alyssa Rhoden, Wade Henning, Ryan
Walker and Tom Neumann for insightful comments and discussions.
NR 38
TC 0
Z9 0
U1 2
U2 10
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0012-821X
EI 1385-013X
J9 EARTH PLANET SC LETT
JI Earth Planet. Sci. Lett.
PD SEP 1
PY 2014
VL 401
BP 275
EP 283
DI 10.1016/j.epsl.2014.05.015
PG 9
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA AO3GV
UT WOS:000341218600025
ER
PT J
AU Kuhn, CE
Baker, JD
Towell, RG
Ream, RR
AF Kuhn, Carey E.
Baker, Jason D.
Towell, Rodney G.
Ream, Rolf R.
TI Evidence of localized resource depletion following a natural
colonization event by a large marine predator
SO JOURNAL OF ANIMAL ECOLOGY
LA English
DT Article
DE Callorhinus ursinus; dive behaviour; foraging behaviour; intraspecific
competition; northern fur seal; satellite telemetry
ID NORTHERN FUR SEALS; CALLORHINUS-URSINUS; PRIBILOF ISLANDS; COLONY SIZE;
GEOGRAPHIC STRUCTURE; FORAGING ENERGETICS; DENSITY-DEPENDENCE; ASHMOLES
HALO; ELEPHANT SEAL; POPULATION
AB 1. For central place foragers, forming colonies can lead to extensive competition for prey around breeding areas and a zone of local prey depletion. As populations grow, this area of reduced prey can expand impacting foraging success and forcing animals to alter foraging behaviour.
2. Here, we examine a population of marine predators, the northern fur seal (Callorhinus ursinus), which colonized a recently formed volcanic island, and assess changes in foraging behaviour associated with increasing population density. Specifically, we measured pup production and adult foraging behaviour over a 15-year period, during which the population increased 4-fold.
3. Using measures of at-sea movements and dive behaviour, we found clear evidence that as the population expanded, animals were required to allot increasing effort to obtain resources. These changes in behaviour included longer duration foraging trips, farther distances travelled, a larger foraging range surrounding the island and deeper maximum dives.
4. Our results suggest that as the northern fur seal population increased, local prey resources were depleted as a result of increased intraspecific competition. In addition, the recent slowing of population growth indicates that this population may be approaching carrying capacity just 31 years after a natural colonization event.
5. Our study offers insight into the dynamics of population growth and impacts of increasing population density on a large marine predator. Such data could be vital for understanding future population fluctuations that occur in response to the dynamic environment, as natural and anthropogenic factors continue to modify marine habitats.
C1 [Kuhn, Carey E.; Towell, Rodney G.; Ream, Rolf R.] NOAA, Natl Marine Mammal Lab, Alaska Fisheries Sci Ctr, Natl Marine Fisheries Serv, Seattle, WA 98115 USA.
[Baker, Jason D.] NOAA, Pacific Isl Fisheries Sci Ctr, Natl Marine Fisheries Serv, Honolulu, HI 96822 USA.
RP Kuhn, CE (reprint author), NOAA, Natl Marine Mammal Lab, Alaska Fisheries Sci Ctr, Natl Marine Fisheries Serv, 7600 Sand Point Way NE, Seattle, WA 98115 USA.
EM Carey.Kuhn@noaa.gov
FU University of Alaska Fairbanks; North Pacific Research Board
FX This research was conducted under Marine Mammal Protection Act permit
numbers 782-1455, 782-1694, 782-1708. A. Banks, K. Call, B. Fadely, T.
Gelatt, J. L. Guerrero, J. Sterling, J. Thomason and M. Williams
assisted with field research. J. Thomason, B. Walker and T. Zeppelin
provided diet analysis, and D. Johnson assisted with statistical
analysis and data processing. Funding and personnel were also
contributed by the University of Alaska Fairbanks and the North Pacific
Research Board. Additional logistic support was provided by R. Brewer,
the US Fish and Wildlife Service (M/V Tiglax), and J. and A. MacDonald.
The findings and conclusions in the study are those of the author(s) and
do not necessarily represent the views of the National Marine Fisheries
Service, NOAA. Reference to trade names does not imply endorsement by
the National Marine Fisheries Service, NOAA.
NR 58
TC 10
Z9 10
U1 3
U2 25
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 0021-8790
EI 1365-2656
J9 J ANIM ECOL
JI J. Anim. Ecol.
PD SEP
PY 2014
VL 83
IS 5
BP 1169
EP 1177
DI 10.1111/1365-2656.12202
PG 9
WC Ecology; Zoology
SC Environmental Sciences & Ecology; Zoology
GA AN8TP
UT WOS:000340877700017
PM 24450364
ER
PT J
AU Frazier, BS
Driggers, WB
Adams, DH
Jones, CM
Loefer, JK
AF Frazier, B. S.
Driggers, W. B., III
Adams, D. H.
Jones, C. M.
Loefer, J. K.
TI Validated age, growth and maturity of the bonnethead Sphyrna tiburo in
the western North Atlantic Ocean
SO JOURNAL OF FISH BIOLOGY
LA English
DT Article
DE longevity; elasmobranch; life history; oxytetracycline
ID GULF-OF-MEXICO; RHIZOPRIONODON-TERRAENOVAE RICHARDSON; SHARPNOSE SHARK;
LIFE-HISTORY; CARCHARHINUS-ACRONOTUS; CHONDRICHTHYAN FISHES; BLACKNOSE
SHARK; 2 POPULATIONS; CONSISTENCY; PRECISION
AB The age, growth and maturity of bonnetheads Sphyrna tiburo inhabiting the estuarine and coastal waters of the western North Atlantic Ocean (WNA) from Onslow Bay, North Carolina, south to West Palm Beach, Florida, were examined. Vertebrae were collected and aged from 329 females and 217 males ranging in size from 262 to 1043 mm and 245 to 825 mm fork length, L-F, respectively. Sex-specific von Bertalanffy growth curves were fitted to length-at-age data. Female von Bertalanffy parameters were L-infinity = 1036 mm L-F, k = 0.18, t(0) = -1.64 and L-0 = 272 mm L-F. Males reached a smaller theoretical asymptotic length and had a higher growth coefficient (L-infinity = 782 mm L-F, k = 0.29, t(0) = -1.43 and L-0 = 266 mm L-F). Maximum observed age was 17.9 years for females and 16.0 years for males. Annual deposition of growth increments was verified by marginal increment analysis and validated for age classes 2.5+ to 10.5+ years through recapture of 13 oxytetracycline-injected specimens at liberty in the wild for 1-4 years. Length (L-F50) and age (A(50)) at 50% maturity were 819 mm and 6.7 years for females, and 618 mm and 3.9 years for males. Both female and male S. tiburo in the WNA had a significantly higher maximum observed age, L-F50, A(50) and L-infinity, and a significantly lower k and estimated L-0 than evident in the Gulf of Mexico (GOM). These significant differences in life-history parameters, as well as evidence from tagging and genetic studies, suggest that S. tiburo in the WNA and GOM should be considered separate stocks. (C) 2014 The Fisheries Society of the British Isles
C1 [Frazier, B. S.] South Carolina Dept Nat Resources, Charleston, SC 29412 USA.
[Driggers, W. B., III; Jones, C. M.] Natl Marine Fisheries Serv, Southeast Fisheries Sci Ctr, Mississippi Labs, Pascagoula, MS 39567 USA.
[Adams, D. H.] Florida Fish & Wildlife Conservat Commiss, Fish & Wildlife Res Inst, Melbourne, FL 32901 USA.
[Loefer, J. K.] Univ S Carolina, Dept Biol Sci, Columbia, SC 29208 USA.
RP Frazier, BS (reprint author), South Carolina Dept Nat Resources, 217 Ft Johnson Rd, Charleston, SC 29412 USA.
EM frazierb@dnr.sc.gov
FU Cooperative Atlantic States Shark Pupping and Nursery Habitat Survey
(COASTSPAN); U.S. Department of the Interior; U.S. Fish and Wildlife
Service; Federal Aid for Sportfish Restoration Project [F-43]; State of
Florida saltwater recreational fishing licence monies
FX We are especially grateful to the many folks who helped make this study
possible. C. Hendrix, J. Richardson, D. Shiffman, H. Davega, J. Tucker,
A. Shaw and P. Webster helped with field work, specimen collection,
workup and vertebrae prepping. We received advice, support and guidance
from many colleagues including: E. Levesque, G. Ulrich, J. Gelsleichter,
J. Carlson, E. Cortes, L. Natanson, J. Neer and C. McCandless. K. Ware
and J. Henne of Bears Bluff National Fish Hatchery were critical to age
validation work. This work was conducted as part of the Master's in
Environmental Science programme at the College of Charleston, and we
thank committee members, A. Strand and S. Arnott as well as directors T.
Callahan and M. McConnell for their support. Funding for this study was
provided by the Cooperative Atlantic States Shark Pupping and Nursery
Habitat Survey (COASTSPAN) and, in part, by funding from the U.S.
Department of the Interior, U.S. Fish and Wildlife Service, Federal Aid
for Sportfish Restoration Project Number F-43 and by State of Florida
saltwater recreational fishing licence monies. Collection of specimens
was performed under SCDNR Scientific Permit #2212, and as such this
study was granted an IACUC exemption. We appreciate the guidance of the
editors and two anonymous reviewers who greatly improved the manuscript.
This is contribution 719 of the South Carolina Marine Resources Center.
NR 52
TC 4
Z9 4
U1 5
U2 30
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 0022-1112
EI 1095-8649
J9 J FISH BIOL
JI J. Fish Biol.
PD SEP
PY 2014
VL 85
IS 3
BP 688
EP 712
DI 10.1111/jfb.12450
PG 25
WC Fisheries; Marine & Freshwater Biology
SC Fisheries; Marine & Freshwater Biology
GA AN8HR
UT WOS:000340845500009
PM 25040650
ER
PT J
AU Gyekenyesi, A
AF Gyekenyesi, Andrew
TI Techniques for monitoring damage in ceramic matrix composites
SO JOURNAL OF INTELLIGENT MATERIAL SYSTEMS AND STRUCTURES
LA English
DT Review
DE Ceramic matrix composite; electrical resistance; cracking;
nondestructive evaluation; damage; ultrasonics; acoustic emissions;
thermography; impedance-based structural health monitoring;
thermoelastic stress analysis
ID ELECTRICAL-RESISTANCE; PULSED THERMOGRAPHY; SENSORS
AB This article offers a review of various nondestructive evaluation and structural health monitoring techniques that have been successfully utilized for assessing the damage state of woven ceramic matrix composites consisting of silicon carbide fibers and silicon carbide matrices. The techniques include acousto-ultrasonics, modal acoustic emissions, electrical resistance, impedance-based structural health monitoring, pulsed thermography, as well as thermoelastic stress analysis. The damage, in the form of distributed matrix cracks and delaminations, was introduced using multiple tactics. These included load/unload/reload uniaxial tensile tests, creep tests, and ballistic impact. Although other nondestructive evaluation techniques have been applied to this material system, the select nondestructive evaluation tools described here are limited to approaches that are of current research interest within programs at the NASA Glenn Research Center.
C1 NASA, Ohio Aerosp Inst, Glenn Res Ctr, Lewis Field, Cleveland, OH 44135 USA.
RP Gyekenyesi, A (reprint author), NASA, Ohio Aerosp Inst, Glenn Res Ctr, Lewis Field, 21000 Brookpk Rd,Mail Stop 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 31
TC 0
Z9 0
U1 3
U2 41
PU SAGE PUBLICATIONS LTD
PI LONDON
PA 1 OLIVERS YARD, 55 CITY ROAD, LONDON EC1Y 1SP, ENGLAND
SN 1045-389X
EI 1530-8138
J9 J INTEL MAT SYST STR
JI J. Intell. Mater. Syst. Struct.
PD SEP
PY 2014
VL 25
IS 13
BP 1531
EP 1540
DI 10.1177/1045389X13510221
PG 10
WC Materials Science, Multidisciplinary
SC Materials Science
GA AN8BV
UT WOS:000340827400001
ER
PT J
AU Taylor, PC
AF Taylor, Patrick C.
TI Variability of Regional TOA Flux Diurnal Cycle Composites at the Monthly
Time Scale
SO JOURNAL OF THE ATMOSPHERIC SCIENCES
LA English
DT Article
ID OUTGOING LONGWAVE RADIATION; HYDROLOGIC-CYCLE; CLOUD COVER; BUDGET;
STRATOCUMULUS; CONVECTION; TROPICS; MODEL; LAYER; CIRCULATION
AB Diurnal variability is a fundamental component of Earth's climate system. Clouds, temperature, and precipitation exhibit robust responses to the daily cycle of solar insolation. Recent work indicates significant variability in the top-of-the-atmosphere (TOA) flux diurnal cycle in the tropics associated with monthly changes in the cloud diurnal cycle evolution. It has been proposed that the observed month-to-month variations in the TOA flux diurnal cycle are caused by anomalies in the atmospheric dynamic and thermodynamic state. This hypothesis is tested using a regression analysis to quantify the relationship between diurnal cycle shape and the atmospheric dynamic and thermodynamic state. TOA radiative fluxes are obtained from Clouds and the Earth's Radiant Energy System (CERES) Edition 3 data and the atmospheric dynamic and thermodynamic state is taken from the European Centre for Medium-Range Weather Forecasts (ECMWF) Interim Re-Analysis. Four regions representing traditional diurnal cycle regimes are used in this analysis: North Africa (land nonconvective), central South America (land convective), Peru marine stratocumulus (ocean nonconvective), and Indian Ocean (ocean convective). The results show a statistically significant diurnal cycle shape change and cloud response related to monthly atmospheric state anomalies. Using the single-variable regression relationships to predict monthly diurnal cycle variability shows improvements of 1%-18% over assuming a climatological diurnal cycle shape; the most significant gains are found in North Africa. The proposed hypothesis, therefore, contributes to diurnal cycle variability explaining at least 10%-20% of the total monthly-mean diurnal cycle variability.
C1 [Taylor, Patrick C.] 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
FU NASA Energy and Water Cycle Study program [NNH10ZDA001N]
FX The author would like to thank the anonymous reviewers for their
insightful comments, which significantly improved the clarity of this
manuscript. This work is supported by the NASA Energy and Water Cycle
Study program through Grant NNH10ZDA001N. The CERES data used in this
study are stored at the Atmospheric Science Data Center at NASA Langley
(https://eosweb.larc.nasa.gov). ERA-Interim data used in this study are
stored at the ECMWF data server
(http://data-portal.ecmwf.int/datald/interim_nmthl).
NR 40
TC 3
Z9 3
U1 0
U2 5
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 SEP
PY 2014
VL 71
IS 9
BP 3484
EP 3498
DI 10.1175/JAS-D-13-0336.1
PG 15
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA AO3KC
UT WOS:000341227100022
ER
PT J
AU Tompson, SR
AF Tompson, Sara R.
TI Predator: The Secret Origins of the Drone Revolution
SO LIBRARY JOURNAL
LA English
DT Book Review
C1 [Tompson, Sara R.] Jet Prop Lab Lib, Pasadena, CA 91109 USA.
RP Tompson, SR (reprint author), Jet Prop Lab Lib, Pasadena, CA 91109 USA.
NR 1
TC 0
Z9 0
U1 1
U2 6
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 SEP 1
PY 2014
VL 139
IS 14
BP 123
EP 124
PG 2
WC Information Science & Library Science
SC Information Science & Library Science
GA AO1MJ
UT WOS:000341075900203
ER
PT J
AU Tompson, SR
AF Tompson, Sara R.
TI The Large Hadron Collider: The Extraordinary Story of the Higgs Boson
and Other Stuff That Will Blow Your Mind
SO LIBRARY JOURNAL
LA English
DT Book Review
C1 [Tompson, Sara R.] Jet Prop Lab Lib, Arch & Records Sect, Pasadena, CA 91109 USA.
RP Tompson, SR (reprint author), Jet Prop Lab Lib, Arch & Records Sect, Pasadena, CA 91109 USA.
NR 1
TC 0
Z9 0
U1 1
U2 4
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 SEP 1
PY 2014
VL 139
IS 14
BP 135
EP +
PG 2
WC Information Science & Library Science
SC Information Science & Library Science
GA AO1MJ
UT WOS:000341075900247
ER
PT J
AU Pfaller, JB
Alfaro-Shigueto, J
Balazs, GH
Ishihara, T
Kopitsky, K
Mangel, JC
Peckham, SH
Bolten, AB
Bjorndal, KA
AF Pfaller, Joseph B.
Alfaro-Shigueto, Joanna
Balazs, George H.
Ishihara, Takashi
Kopitsky, Kerry
Mangel, Jeffrey C.
Peckham, S. Hoyt
Bolten, Alan B.
Bjorndal, Karen A.
TI Hitchhikers reveal cryptic host behavior: new insights from the
association between Planes major and sea turtles in the Pacific Ocean
SO MARINE BIOLOGY
LA English
DT Article
ID CENTRAL NORTH PACIFIC; FEEDING HABITAT USE; CARETTA-CARETTA;
LEPIDOCHELYS-OLIVACEA; CHELONIA-MYDAS; LOGGERHEAD TURTLES; COLUMBUS
CRABS; SATELLITE TELEMETRY; CARAPACE EPIBIONTS; DEPTH DISTRIBUTION
AB Studies that incorporate information from habitat-specific ecological interactions (e.g., epibiotic associations) can reveal valuable insights into the cryptic habitat-use patterns and behavior of marine vertebrates. Sea turtles, like other large, highly mobile marine vertebrates, are inherently difficult to study, and such information can inform the implementation of conservation measures. The presence of epipelagic epibionts, such as the flotsam crab Planes major, on sea turtles strongly suggests that neritic turtles have recently occupied epipelagic habitats (upper 200 m in areas with > 200 m depth) and that epipelagic turtles spend time at or near the surface. We quantified the effects of turtle species, turtle size, and habitat (neritic or epipelagic) on the frequency of epibiosis (F (0)) by P. major on sea turtles in the Pacific Ocean. In neritic habitats, we found that loggerhead (F (0) = 27.6 %) and olive ridley turtles (F (0) = 26.2 %) host crabs frequently across a wide range of body sizes, and green turtles almost never host crabs (F (0) = 0.7 %). These results suggest that loggerheads and olive ridleys display variable/flexible epipelagic-neritic transitions, while green turtles tend to transition unidirectionally at small body sizes. In epipelagic habitats, we found that loggerheads host crabs (F (0) = 92.9 %) more frequently than olive ridleys (F (0) = 50 %) and green turtles (F (0) = 38.5 %). These results suggest that epipelagic loggerheads tend to spend more time at or near the surface than epipelagic olive ridleys and green turtles. Results of this study reveal new insights into habitat-use patterns and behavior of sea turtles and display how epibiont data can supplement data from more advanced technologies to gain a better understanding of the ecology of marine vertebrates during cryptic life stages.
C1 [Pfaller, Joseph B.; Bolten, Alan B.; Bjorndal, Karen A.] Univ Florida, Archie Carr Ctr Sea Turtle Res, Dept Biol, Gainesville, FL 32611 USA.
[Pfaller, Joseph B.] Caretta Res Project, Savannah, GA 31412 USA.
[Alfaro-Shigueto, Joanna; Mangel, Jeffrey C.] ProDelphinus, Lima 630204 18, Peru.
[Alfaro-Shigueto, Joanna; Mangel, Jeffrey C.] Univ Exeter, Ctr Ecol & Conservat, Penryn TR10 9EZ, Cornwall, England.
[Balazs, George H.] NOAA, Marine Turtle Res Program, Natl Marine Fisheries Serv, Pacific Isl Fisheries Sci Ctr, Honolulu, HI 96818 USA.
[Ishihara, Takashi] Sea Turtle Assoc Japan, Osaka, Japan.
[Ishihara, Takashi] Suma Aqualife Pk, Kobe, Hyogo, Japan.
[Kopitsky, Kerry] Rising Tides Restorat, Dover, DE 19904 USA.
[Peckham, S. Hoyt] Stanford Univ, Ctr Ocean Solut, Pacific Grove, CA 93950 USA.
RP Pfaller, JB (reprint author), Univ Florida, Archie Carr Ctr Sea Turtle Res, Dept Biol, Gainesville, FL 32611 USA.
EM jpfaller@ufl.edu
OI Bjorndal, Karen/0000-0002-6286-1901
NR 62
TC 3
Z9 3
U1 3
U2 20
PU SPRINGER HEIDELBERG
PI HEIDELBERG
PA TIERGARTENSTRASSE 17, D-69121 HEIDELBERG, GERMANY
SN 0025-3162
EI 1432-1793
J9 MAR BIOL
JI Mar. Biol.
PD SEP
PY 2014
VL 161
IS 9
BP 2167
EP 2178
DI 10.1007/s00227-014-2498-3
PG 12
WC Marine & Freshwater Biology
SC Marine & Freshwater Biology
GA AN8QT
UT WOS:000340869600017
ER
PT J
AU Inoue, M
Matheou, G
Teixeira, J
AF Inoue, M.
Matheou, G.
Teixeira, J.
TI LES of a Spatially Developing Atmospheric Boundary Layer: Application of
a Fringe Method for the Stratocumulus to Shallow Cumulus Cloud
Transition
SO MONTHLY WEATHER REVIEW
LA English
DT Article
ID LARGE-EDDY SIMULATION; SEA-SURFACE TEMPERATURE; SUBGRID-STRESS MODEL;
NUMERICAL-SIMULATION; FLOW
AB An arrangement of a large-eddy simulation (LES) is described that facilitates a spatially developing thermally stratified atmospheric boundary layer (ABL). When the inflow and outflow boundary conditions are specified, the LES of stably stratified ABL turns out to be challenging because spurious reflections of waves at the boundary accumulate inside the domain. To tackle this problem, a fringe method with an auxiliary LES running concurrently is applied to enforce upstream/downstream boundary conditions. An artificial forcing term is applied within a fringe region located at the beginning of the main LES domain in order to ensure statistically stationary inflow boundary conditions. The auxiliary LES, which is horizontally homogeneous in a doubly periodic domain, is used to determine the inflow condition of the main LES domain. The present scheme is used to provide an Eulerian perspective of the stratocumulus to shallow cumulus cloud (Sc-Cu) transition, one of the key cloud regimes over the subtropical ocean. In this study, the transition is triggered by increasing the sea surface temperature (SST) and the LES runs until a statistically steady evolution of the Sc-Cu transition is achieved. The flow statistics are compared with those from a recycling-type method and it is found that the fringe method is more suitable for the current applications.
C1 [Inoue, M.; Matheou, G.; Teixeira, J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Inoue, M (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM michio.inoue@jpl.nasa.gov
FU Office of Naval Research, Marine Meteorology Program [N00014111P20087,
N0001411IP20069]; NASA MAP Program; NOAA/CPO MAPP Program
FX The authors acknowledge the support provided by the Office of Naval
Research, Marine Meteorology Program under Awards N00014111P20087 and
N0001411IP20069, the NASA MAP Program, and the NOAA/CPO MAPP Program.
Helpful discussions with K. Suselj and K. Suzuki (JPL) are also greatly
acknowledged. 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 32
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U1 0
U2 7
PU AMER METEOROLOGICAL SOC
PI BOSTON
PA 45 BEACON ST, BOSTON, MA 02108-3693 USA
SN 0027-0644
EI 1520-0493
J9 MON WEATHER REV
JI Mon. Weather Rev.
PD SEP
PY 2014
VL 142
IS 9
BP 3418
EP 3424
DI 10.1175/MWR-D-13-00400.1
PG 7
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA AO2QU
UT WOS:000341171100021
ER
PT J
AU Smith, SM
Castaneda-Sceppa, C
O'Brien, KO
Abrams, SA
Gillman, P
Brooks, NE
Cloutier, GJ
Heer, M
Zwart, SR
Wastney, ME
AF Smith, S. M.
Castaneda-Sceppa, C.
O'Brien, K. O.
Abrams, S. A.
Gillman, P.
Brooks, N. E.
Cloutier, G. J.
Heer, M.
Zwart, S. R.
Wastney, M. E.
TI Calcium kinetics during bed rest with artificial gravity and exercise
countermeasures
SO OSTEOPOROSIS INTERNATIONAL
LA English
DT Article
DE Biochemical markers of bone turnover; Exercise; Microgravity; Nutrition;
Space flight
ID INDUCED BONE LOSS; AMINO-ACID SUPPLEMENTATION; RESISTANCE EXERCISE;
SPACE-FLIGHT; ENERGY DEFICIT; METABOLISM; SPACEFLIGHT; WEIGHTLESSNESS;
RESORPTION; RECOVERY
AB We assessed the potential for countermeasures to lessen the loss of bone calcium during bed rest. Subjects ingested less calcium during bed rest, and with artificial gravity, they also absorbed less calcium. With exercise, they excreted less calcium. To retain bone during bed rest, calcium intake needs to be maintained.
This study aims to assess the potential for artificial gravity (AG) and exercise (EX) to mitigate loss of bone calcium during space flight.
We performed two studies: (1) a 21-day bed rest (BR) study with subjects receiving 1 h/day AG (n = 8) or no AG (n = 7) and (2) a 28-day BR study with 1 h/day resistance EX (n = 10) or no EX (n = 3). In both studies, stable isotopes of Ca were administered orally and intravenously, at baseline and after 10 days of BR, and blood, urine, and feces were sampled for up to 14 days post dosing. Tracers were measured using thermal ionization mass spectrometry. Data were analyzed by compartmental modeling.
Less Ca was absorbed during BR, resulting in lower Ca balance in BR+AG (-6.04 +/- 3.38 mmol/day, P = 0.023). However, Ca balance did not change with BR+EX, even though absorbed Ca decreased and urinary Ca excretion increased, because endogenous excretion decreased, and there was a trend for increased bone deposition (P = 0.06). Urinary N-telopeptide excretion increased in controls during BR, but not in the EX group. Markers of bone formation were not different between treatment groups for either study. Ca intake decreased during BR (by 5.4 mmol/day in the AG study and 2.8 mmol/day in the EX study), resulting in lower absorbed Ca.
During BR (or space flight), Ca intake needs to be maintained or even increased with countermeasures such as exercise, to enable maintenance of bone Ca.
C1 [Smith, S. M.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA.
[Castaneda-Sceppa, C.; Cloutier, G. J.] Northeastern Univ, Boston, MA 02115 USA.
[O'Brien, K. O.] Cornell Univ, Ithaca, NY USA.
[Abrams, S. A.] ARS, Baylor Coll Med, USDA, Childrens Nutr Res Ctr, Houston, TX USA.
[Gillman, P.] EASI, Houston, TX USA.
[Brooks, N. E.] Univ Stirling, Stirling FK9 4LA, Scotland.
[Heer, M.] Univ Bonn, Bonn, Germany.
[Zwart, S. R.] Univ Space Res Assoc, Houston, TX USA.
[Wastney, M. E.] Metab Modeling, W Lafayette, IN USA.
RP Smith, SM (reprint author), NASA, Lyndon B Johnson Space Ctr, Attn Mail Code SK3,2101 NASA Pkwy, Houston, TX 77058 USA.
EM scott.m.smith@nasa.gov
OI Abrams, Steven/0000-0003-4972-9233
FU NASA Flight Analogs Project of NASA's Human Research Program; National
Center for Advancing Translational Sciences, National Institutes of
Health [1UL1RR029876-01]; National Space Biomedical Research Institute
(NSBRI) [NCC 9-58]; U.S. Department of Agriculture's Agricultural
Research Service [58-1950-9-001]; National Institutes of Health GCRC
[M01-RR-000054]
FX We thank the subjects for their time and willingness to participate in
these studies. We thank the staff of the UTMB Institute for
Translational Sciences Clinical Research Center for their assistance
with the AG study and the Tufts University GCRC for their support in
conducting the exercise study. We thank the staff of the U.S. National
Aeronautics and Space Administration (NASA) Johnson Space Center
Nutritional Biochemistry Laboratory for their assistance in processing
and analyzing the samples and in all aspects of carrying out this
project. We thank Jane Krauhs for editorial assistance. The AG study was
funded in part by the NASA Flight Analogs Project of NASA's Human
Research Program and in part by grant 1UL1RR029876-01 from the National
Center for Advancing Translational Sciences, National Institutes of
Health. The exercise study was supported by the National Space
Biomedical Research Institute (NSBRI) through NCC 9-58, by agreement
58-1950-9-001 from the U.S. Department of Agriculture's Agricultural
Research Service, and by a grant M01-RR-000054 from the National
Institutes of Health GCRC.
NR 26
TC 2
Z9 2
U1 2
U2 7
PU SPRINGER LONDON LTD
PI LONDON
PA 236 GRAYS INN RD, 6TH FLOOR, LONDON WC1X 8HL, ENGLAND
SN 0937-941X
EI 1433-2965
J9 OSTEOPOROSIS INT
JI Osteoporosis Int.
PD SEP
PY 2014
VL 25
IS 9
BP 2237
EP 2244
DI 10.1007/s00198-014-2754-x
PG 8
WC Endocrinology & Metabolism
SC Endocrinology & Metabolism
GA AN6AK
UT WOS:000340675200010
PM 24861908
ER
PT J
AU Cheung, KC
Tachi, T
Calisch, S
Miura, K
AF Cheung, Kenneth C.
Tachi, Tomohiro
Calisch, Sam
Miura, Koryo
TI Origami interleaved tube cellular materials
SO SMART MATERIALS AND STRUCTURES
LA English
DT Article
DE rigid origami; metametrial; cellular structure; dimensional scaling
analysis
AB A novel origami cellular material based on a deployable cellular origami structure is described. The structure is bi-directionally flat-foldable in two orthogonal (x and y) directions and is relatively stiff in the third orthogonal (z) direction. While such mechanical orthotropicity is well known in cellular materials with extruded two dimensional geometry, the interleaved tube geometry presented here consists of two orthogonal axes of interleaved tubes with high interfacial surface area and relative volume that changes with fold-state. In addition, the foldability still allows for fabrication by a flat lamination process, similar to methods used for conventional expanded two dimensional cellular materials. This article presents the geometric characteristics of the structure together with corresponding kinematic and mechanical modeling, explaining the orthotropic elastic behavior of the structure with classical dimensional scaling analysis.
C1 [Cheung, Kenneth C.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Tachi, Tomohiro] Univ Tokyo, Dept Gen Syst Studies, Meguro Ku, Tokyo 1538902, Japan.
[Calisch, Sam] MIT, Ctr Bits & Atoms, Cambridge, MA 02139 USA.
[Miura, Koryo] Univ Tokyo, Tokyo 1538902, Japan.
RP Cheung, KC (reprint author), NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
EM kenneth.c.cheung@nasa.gov; tachi@idea.c.u-tokyo.ac.jp;
sam.calisch@cba.mit.edu; miurak@gakushikai.jp
FU NASA Ames Research Center; University of Tokyo; MIT Center for Bits and
Atoms; NASA STMD Center Innovation Fund; JST Presto Program
FX The authors would like to acknowledge the support of the NASA Ames
Research Center, the University of Tokyo, and the MIT Center for Bits
and Atoms. The first author's contributions were supported by the NASA
STMD Center Innovation Fund. The second author is supported by the JST
Presto Program.
NR 26
TC 14
Z9 14
U1 0
U2 14
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0964-1726
EI 1361-665X
J9 SMART MATER STRUCT
JI Smart Mater. Struct.
PD SEP
PY 2014
VL 23
IS 9
AR 094012
DI 10.1088/0964-1726/23/9/094012
PG 10
WC Instruments & Instrumentation; Materials Science, Multidisciplinary
SC Instruments & Instrumentation; Materials Science
GA AO1MX
UT WOS:000341077700014
ER
PT J
AU Peng, TS
Saxena, A
Goebel, K
Xiang, YB
Liu, YM
AF Peng, Tishun
Saxena, Abhinav
Goebel, Kai
Xiang, Yibing
Liu, Yongming
TI Integrated experimental and numerical investigation for fatigue damage
diagnosis in composite plates
SO STRUCTURAL HEALTH MONITORING-AN INTERNATIONAL JOURNAL
LA English
DT Article
DE Composite; Lamb wave; delamination; matrix cracking; finite element
model
ID LAMB WAVE-PROPAGATION; SIMULATION
AB An integrated experimental and numerical investigation of fatigue damage diagnosis in composite plates is presented in this study. First, the fatigue testing setup for carbon-carbon composite coupons is described with corresponding health monitoring approach through Lamb wave-based diagnostic data collection. In order to study the effects of degradation evolution, a finite element model is used to simulate the effect on Lamb wave propagation due to fatigue-induced delamination and matrix cracking. Simulation results are compared with the experimental testing to first validate the model and then develop several features as potential damage indicators. A parametric study is conducted on the effects of varying degrees of delamination and matrix cracking on these features. Results from the model simulations are presented along with the data analysis and discussions on the capability and limitations of the approach. Finally, some conclusions are drawn and future work is proposed based on the results obtained so far.
C1 [Peng, Tishun; Xiang, Yibing; Liu, Yongming] Arizona State Univ, Sch Engn Matter Transport & Energy, Tempe, AZ 85287 USA.
[Saxena, Abhinav] NASA, SGT, Ames Res Ctr, Moffett Field, CA USA.
[Goebel, Kai] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
RP Liu, YM (reprint author), Arizona State Univ, Sch Engn Matter Transport & Energy, Tempe, AZ 85287 USA.
EM yongming.liu@asu.edu
FU National Aeronautical and Space Administration (NASA) through Global
Engineering and Materials, Inc. (GEM) [NNX12CA86C]
FX The research reported in this article was partially supported by the
National Aeronautical and Space Administration (NASA) through Global
Engineering and Materials, Inc. (GEM) under the project NNX12CA86C.
NR 27
TC 1
Z9 1
U1 0
U2 6
PU SAGE PUBLICATIONS LTD
PI LONDON
PA 1 OLIVERS YARD, 55 CITY ROAD, LONDON EC1Y 1SP, ENGLAND
SN 1475-9217
EI 1741-3168
J9 STRUCT HEALTH MONIT
JI Struct. Health Monit.
PD SEP
PY 2014
VL 13
IS 5
BP 537
EP 547
DI 10.1177/1475921714532992
PG 11
WC Engineering, Multidisciplinary; Instruments & Instrumentation
SC Engineering; Instruments & Instrumentation
GA AO2WP
UT WOS:000341187700004
ER
PT J
AU Stebner, AP
Bigelow, GS
Yang, J
Shukla, DP
Saghaian, SM
Rogers, R
Garg, A
Karaca, HE
Chumlyakov, Y
Bhattacharya, K
Noebe, RD
AF Stebner, Aaron P.
Bigelow, Glen S.
Yang, Jin
Shukla, Dhwanil P.
Saghaian, Sayed M.
Rogers, Richard
Garg, Anita
Karaca, Haluk E.
Chumlyakov, Yuriy
Bhattacharya, Kaushik
Noebe, Ronald D.
TI Transformation strains and temperatures of a nickel-titanium-hafnium
high temperature shape memory alloy
SO ACTA MATERIALIA
LA English
DT Article
DE Orientation; Texture; Precipitates; Grain boundaries; Transformation
strain
ID NI SINGLE-CRYSTALS; MARTENSITIC-TRANSFORMATION; YIELD SURFACE; TEXTURE;
TENSION; PHASE; MICROSTRUCTURE; POLYCRYSTALS; COMPRESSION; BEHAVIOR
AB A combined experimental and theoretical investigation of the transformation temperature and transformation strain behaviors of a promising new Ni50.3Ti29.7Hf20 high-temperature shape memory alloy was conducted. Actuation behavior of single crystals with loading orientations near [0 0 1](B2), [(1) over bar 1 0](B2), and [1 1 1](B2), as well as polycrystalline material in aged and unaged conditions was studied, together with the superelastic, polycrystalline torsion response. These results were compared to analytic calculations of the ideal transformation strains for tension, compression, and torsion loading of single crystals as a function of single crystal orientation, and polycrystalline material of common processing textures. H-phase precipitates on the order of 10-30 nm were shown to increase transformation temperatures and also to narrow thermal hysteresis, compared to unaged material. The mechanical effects of increased residual stresses and numbers of transformation nucleation sites caused by the precipitates provide a plausible explanation for the observed transformation temperature trends. Grain boundaries were shown to have similar effects on transformation temperatures. The work output and recoverable strain exhibited by the alloy were shown to approach maximums at stresses of 500-800 MPa, suggesting these to be optimal working loads with respect to single cycle performance. The potential for transformation strain in single crystals of this material was calculated to be superior to binary NiTi in tension, compression, and torsion loading modes. However, the large volume fraction of precipitate phase, in part, prevents the material from realizing its full single crystal transformation strain potential in return for outstanding functional stability by inhibiting plastic strain accumulation during transformation. Finally, calculations showed that of the studied polycrystalline textures, [0 0 1](B2) fiber texture results in superior torsion performance, while [0 1 1](B2) fiber texture results in superior tensile behavior, and both [0 1 1](B2) and random textures will result in the best possible compression performance. (C) 2014 Acta Materialia Inc. Published by Elsevier Ltd. All rights reserved.
C1 [Stebner, Aaron P.; Yang, Jin; Shukla, Dhwanil P.; Bhattacharya, Kaushik] CALTECH, Pasadena, CA 91125 USA.
[Bigelow, Glen S.; Rogers, Richard; Noebe, Ronald D.] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA.
[Saghaian, Sayed M.; Karaca, Haluk E.] Univ Kentucky, Lexington, KY 40506 USA.
[Garg, Anita] Univ Toledo, Toledo, OH 43606 USA.
[Chumlyakov, Yuriy] Tomsk State Univ, Siberian Phys Tech Inst, Tomsk 634050, Russia.
RP Stebner, AP (reprint author), Colorado Sch Mines, 1610 Illinois St, Golden, CO 80401 USA.
EM astebner@mines.edu
RI Stebner, Aaron/A-7685-2015; Chumlyakov, Yuriy/R-6496-2016
FU NASA's Fundamental Aeronautics Program, Aeronautical Sciences Project;
California Institute of Technology Summer Undergraduate Research
Fellowship; Tsien fellowship at the California Institute of Technology
FX This work was supported by NASA's Fundamental Aeronautics Program,
Aeronautical Sciences Project. D.P.S. acknowledges the support of a
California Institute of Technology Summer Undergraduate Research
Fellowship. J.Y. acknowledges a Tsien fellowship that supported his
undergraduate research at the California Institute of Technology.
NR 50
TC 11
Z9 12
U1 9
U2 43
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 1359-6454
EI 1873-2453
J9 ACTA MATER
JI Acta Mater.
PD SEP 1
PY 2014
VL 76
BP 40
EP 53
DI 10.1016/j.actamat.2014.04.071
PG 14
WC Materials Science, Multidisciplinary; Metallurgy & Metallurgical
Engineering
SC Materials Science; Metallurgy & Metallurgical Engineering
GA AN1GJ
UT WOS:000340330400004
ER
PT J
AU Nesbitt, JA
AF Nesbitt, James A.
TI Rate of Sublimation of Yb14MnSb11, a Thermoelectric Material for Space
Power Applications
SO JOURNAL OF ELECTRONIC MATERIALS
LA English
DT Article
DE Zintl; Yb14MnSb11; sublimation; Yb2O3; oxidation
ID PERFORMANCE; OXIDATION; YB14MN1-XALXSB11; YB14-XCAXMNSB11; TRANSITION;
EFFICIENCY; CORROSION; ALLOYS
AB The compound Yb14MnSb11 is a p-type thermoelectric material of interest for space power applications. However, average rates of sublimation previously measured at 1000A degrees C were unacceptably high. In at least one study, Yb2O3 was observed on the surface after testing. In this study, the rate of sublimation of Yb14MnSb11 was measured at 1000A degrees C by use of a vacuum thermogravimetric analyzer (TGA) which continuously measures weight loss as a result of sublimation. This experiment revealed that the rate of sublimation decreased with time, but also resulted in formation of Yb2O3 on the surface, even though the base pressure at the start of the test was 1.9 x 10(-4) Pa (1.4 x 10(-6) torr). Subsequently, the effect of the Yb2O3 on the rate of sublimation was evaluated by performing interrupted vacuum furnace tests in which the sample was weighed after exposure at 1000A degrees C for different times. During the weighing periods, the accumulated oxide scale was either completely removed or left to accumulate further on the surface. The interrupted furnace tests showed that formation of Yb2O3 on the surface was the likely cause of the reduction in the rate of sublimation of the Yb14MnSb11 when measured by use of the vacuum TGA, at least for the measured test duration. Therefore, uncoated material in the vacuum of space, where oxygen is absent, would be likely to sublime at a continuous rate in excess of 5 x 10(-3) g/cm(2)/h.
C1 NASA, Glenn Res Ctr, Cleveland, OH 44135 USA.
RP Nesbitt, JA (reprint author), NASA, Glenn Res Ctr, Cleveland, OH 44135 USA.
EM JNesbitt@nasa.gov
FU Radioisotope Power Systems Office at the NASA Glenn Research Center
under the Technology Advancement Project, Advanced Thermoelectric Couple
(ATEC) Program
FX Supply of the Yb14MnSb11 material by the Jet
Propulsion Laboratory in Pasadena, CA,, USA, is gratefully acknowledged.
This work was funded by the Radioisotope Power Systems Office at the
NASA Glenn Research Center under the Technology Advancement Project,
Advanced Thermoelectric Couple (ATEC) Program.
NR 29
TC 3
Z9 3
U1 3
U2 20
PU SPRINGER
PI NEW YORK
PA 233 SPRING ST, NEW YORK, NY 10013 USA
SN 0361-5235
EI 1543-186X
J9 J ELECTRON MATER
JI J. Electron. Mater.
PD SEP
PY 2014
VL 43
IS 9
BP 3128
EP 3137
DI 10.1007/s11664-014-3261-8
PG 10
WC Engineering, Electrical & Electronic; Materials Science,
Multidisciplinary; Physics, Applied
SC Engineering; Materials Science; Physics
GA AN1SJ
UT WOS:000340363600010
ER
PT J
AU Skonieczny, K
Moreland, SJ
Asnani, VM
Creager, CM
Inotsume, H
Wettergreen, DS
AF Skonieczny, Krzysztof
Moreland, Scott J.
Asnani, Vivake M.
Creager, Colin M.
Inotsume, Hiroaki
Wettergreen, David S.
TI Visualizing and Analyzing Machine-soil Interactions using Computer
Vision
SO JOURNAL OF FIELD ROBOTICS
LA English
DT Article
ID BEHAVIOR; MOTION; SCALE; FIELD; FLOW
AB This work presents an experimental method for visualizing and analyzing machine-soil interactions, namely the soil optical flow technique (SOFT). SOFT uses optical flow and clustering techniques to process images of soil interacting with a wheel or tool from photos taken through a glass wall of a soil bin. It produces results that are far richer than past approaches that utilized long-exposure photography. It achieves a performance comparable to particle image velocimetry or particle tracking velocimetry, but without the need for specialized measurement equipment or specially marked soil particles. The processing technique demonstrates robustness to different soil types. Ground-truth and cross-validation experiments exhibit subpixel accuracy in estimating soil motions. An example of an application of this technique for field robotics research is the detailed study of push-rolling for slope climbing and soft soil traverse. Push-rolling advances a vehicle by rolling a subset of its wheels while changing its wheelbase to keep the other wheels static and pushing against the ground. Experiments show that push-rolling achieves higher net traction than conventional rolling. Observing the two aspects of push-rolling (rolling and horizontal pushing) using SOFT shows that they result in entirely different forms of soil shearing ("grip failure" and "ground failure," respectively). SOFT also demonstrates how the direction of soil motion is more efficiently utilized for horizontal thrust by pushing than conventional rolling. Ongoing work utilizing SOFT has also demonstrated its potential use in studying excavation tool interactions, the effects of grousers on wheel efficiency, as well as a variety of other wheel-soil interactions. (C) 2014 Wiley Periodicals, Inc.
C1 [Skonieczny, Krzysztof; Moreland, Scott J.] Carnegie Mellon Univ, Field Robot Ctr, Pittsburgh, PA 15213 USA.
[Asnani, Vivake M.; Creager, Colin M.] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA.
[Inotsume, Hiroaki; Wettergreen, David S.] Carnegie Mellon Univ, Field Robot Ctr, Pittsburgh, PA 15213 USA.
RP Skonieczny, K (reprint author), Carnegie Mellon Univ, Field Robot Ctr, 5000 Forbes Ave, Pittsburgh, PA 15213 USA.
EM kskoniec@cmu.edu
NR 28
TC 5
Z9 5
U1 1
U2 14
PU WILEY
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 1556-4959
EI 1556-4967
J9 J FIELD ROBOT
JI J. Field Robot.
PD SEP-OCT
PY 2014
VL 31
IS 5
SI SI
BP 753
EP 769
DI 10.1002/rob.21510
PG 17
WC Robotics
SC Robotics
GA AN2PF
UT WOS:000340427100003
ER
PT J
AU Punge, HJ
Bedka, KM
Kunz, M
Werner, A
AF Punge, H. J.
Bedka, K. M.
Kunz, M.
Werner, A.
TI A new physically based stochastic event catalog for hail in Europe
SO NATURAL HAZARDS
LA English
DT Article
DE Hail; Climatology; Overshooting top; Europe
ID DEEP CONVECTIVE CLOUDS; SATELLITE-OBSERVATIONS; SIZE DISTRIBUTIONS;
SEVERE HAILSTORMS; KINETIC-ENERGY; CLIMATOLOGY; RADAR; DAMAGE; STORM;
TOP
AB Hailstorms represent one of the major sources of damage and insurance loss to residential, commercial, and agricultural assets in several parts of Central Europe. However, there is little knowledge of hail risk across Europe beyond local historical damage reports due to the relative rarity of severe hail events and the lack of uniform detection methods. Here we present a new stochastic catalog of hailstorms for Europe. It is based on satellite observations of overshooting cloud tops (OT) that indicate very strong convective updrafts and hail reports from the European Severe Weather Database (ESWD). Historic hail events are defined based on OT detections from satellite infrared brightness temperatures between 2004 and 2011 for the warm seasons (April-September). The satellite-based historical event properties are complemented by hailstone observations from ESWD to stochastically simulate more than 1 million individual events with an event footprint resolution of 10 km. The final hail event catalog presented in this paper is the first one with a spatial event distribution that is based on a single homogeneous observation source over Europe. Areas of high hail probability or hail risk are found over Central and Southern Europe, including mountainous regions such as the Alps or the Pyrenees. Another region of relatively high hail risk is present over central Eastern Europe.
C1 [Punge, H. J.; Kunz, M.] Karlsruhe Inst Technol, Inst Meteorol & Climate Res, D-76021 Karlsruhe, Germany.
[Punge, H. J.] Willis Ltd, Willis Res Network, London, England.
[Bedka, K. M.] NASA, Langley Res Ctr, Sci Directorate, Hampton, VA 23665 USA.
[Werner, A.] Willis Re GmbH & Co KG, Munich, Germany.
RP Punge, HJ (reprint author), Karlsruhe Inst Technol, Inst Meteorol & Climate Res, D-76021 Karlsruhe, Germany.
EM punge@kit.edu
RI Kunz, Michael/B-1186-2013
FU Willis as part of Willis Research Network (WRN); Center for Disaster
Management and Risk Reduction Technology (CEDIM)
FX H.J.P. was funded as part of his Research Fellowship by Willis as part
of Willis Research Network (WRN). The Center for Disaster Management and
Risk Reduction Technology (CEDIM) supports the research on natural
hazards at the Karlsruhe Institute of Technology (KIT) and the German
Research Center for Geosciences (GFZ). The authors thank ESWD, European
Severe Weather Database (eswd.eu) for providing hail report data. The
authors also thank the GOES-R Algorithm Working Group for support in the
development of the objective overshooting convective cloud top detection
algorithm. The comments of two anonymous reviewers helped to improve
this manuscript.
NR 77
TC 11
Z9 11
U1 3
U2 15
PU SPRINGER
PI NEW YORK
PA 233 SPRING ST, NEW YORK, NY 10013 USA
SN 0921-030X
EI 1573-0840
J9 NAT HAZARDS
JI Nat. Hazards
PD SEP
PY 2014
VL 73
IS 3
BP 1625
EP 1645
DI 10.1007/s11069-014-1161-0
PG 21
WC Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences;
Water Resources
SC Geology; Meteorology & Atmospheric Sciences; Water Resources
GA AN3MQ
UT WOS:000340492700026
ER
PT J
AU Brown, ME
Grace, K
Shively, G
Johnson, KB
Carroll, M
AF Brown, Molly E.
Grace, Kathryn
Shively, Gerald
Johnson, Kiersten B.
Carroll, Mark
TI Using satellite remote sensing and household survey data to assess human
health and nutrition response to environmental change
SO POPULATION AND ENVIRONMENT
LA English
DT Article
DE DHS; NDVI; Environment; Health; Survey; Nutrition
ID NET PRIMARY PRODUCTION; LAND DEGRADATION; FOOD SECURITY; MODIS DATA;
CLIMATE; BIODIVERSITY; AVHRR; NDVI; AGRICULTURE; SEASONALITY
AB Climate change and degradation of ecosystem services functioning may threaten the ability of current agricultural systems to keep up with demand for adequate and inexpensive food and for clean water, waste disposal and other broader ecosystem services. Human health is likely to be affected by changes occurring across multiple geographic and time scales. Impacts range from increasing transmissibility and the range of vectorborne diseases, such as malaria and yellow fever, to undermining nutrition through deleterious impacts on food production and concomitant increases in food prices. This paper uses case studies to describe methods that make use of satellite remote sensing and Demographic and Health Survey data to better understand individual-level human health and nutrition outcomes. By bringing these diverse datasets together, the connection between environmental change and human health outcomes can be described through new research and analysis.
C1 [Brown, Molly E.] NASA, Goddard Space Flight Ctr, Biospher Sci Lab, Greenbelt, MD 20771 USA.
[Grace, Kathryn] Univ Utah, Salt Lake City, UT 84112 USA.
[Shively, Gerald] Purdue Univ, W Lafayette, IN 47907 USA.
[Shively, Gerald] Norwegian Univ Life Sci, Dept Econ & Resource Management, N-1432 As, Norway.
[Johnson, Kiersten B.] Westat Corp, Rockville, MD 20850 USA.
[Carroll, Mark] NASA, Goddard Space Flight Ctr, Sigma Space Corp, Greenbelt, MD 20771 USA.
RP Brown, ME (reprint author), NASA, Goddard Space Flight Ctr, Biospher Sci Lab, Code 618, Greenbelt, MD 20771 USA.
EM molly.e.brown@nasa.gov
RI Brown, Molly/E-2724-2010
OI Brown, Molly/0000-0001-7384-3314
NR 67
TC 10
Z9 10
U1 2
U2 32
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0199-0039
EI 1573-7810
J9 POPUL ENVIRON
JI Popul. Env.
PD SEP
PY 2014
VL 36
IS 1
BP 48
EP 72
DI 10.1007/s11111-013-0201-0
PG 25
WC Demography; Environmental Studies
SC Demography; Environmental Sciences & Ecology
GA AN4NZ
UT WOS:000340566100003
ER
PT J
AU Maynard, DJ
Trial, JG
AF Maynard, Desmond J.
Trial, Joan G.
TI The use of hatchery technology for the conservation of Pacific and
Atlantic salmon
SO REVIEWS IN FISH BIOLOGY AND FISHERIES
LA English
DT Article
DE Salmon; Oncorhynchus; Salmo salar; Conservation; Hatchery
ID COLUMBIA-RIVER; BIOECONOMIC CONTRIBUTION; WILD POPULATIONS; COHO SALMON;
FISHERIES; SALAR; ENHANCEMENT; WASHINGTON; ISSUES; BROODS
AB Hatchery technology has been employed for the conservation of Pacific (Oncorhynchus spp.) and Atlantic salmon (Salmo salar) for over 140 years. The initial societal paradigm was that nature is inefficient and hatcheries could be used to conserve stocks that were over utilized or suffering habitat degradation. Although these early hatcheries failed to meet their conservation objectives, they succeeded in developing the spawning-to-swimup fry culture technology used today. In the 1930s the paradigm shifted to artificial and natural production being equally effective and led to the closure of Federal hatcheries in areas with intact freshwater habitat. Hatcheries were maintained to mitigate for habitat loss from hydropower development. With the development of cost effective smolt production technology by 1960, the paradigm returned to nature being inefficient and ushered in the massive conservation utilization production of Pacific salmon that continues to this day. The early 1990s saw another paradigm shift with nature's inefficiency recognized as being the foundation for evolution to maintain the fitness of salmon in their natural environment. This shift gave rise to a focus for hatchery technology to preserve stocks in their native habitats. Using hatcheries for preservation-conservation has become the norm for Atlantic salmon in the USA and Atlantic Canada and for Pacific salmon stocks listed under the Endangered Species Act in the USA or as species at risk in Canada.
C1 [Maynard, Desmond J.] NOAA, Resource Utilizat & Technol Div, NW Fisheries Sci Ctr, Natl Marine Fisheries Serv, Manchester, WA 98353 USA.
[Trial, Joan G.] Maine Dept Marine Resources, Div Sea Run Fisheries & Habitat, Bangor, ME USA.
RP Maynard, DJ (reprint author), NOAA, Resource Utilizat & Technol Div, NW Fisheries Sci Ctr, Natl Marine Fisheries Serv, POB 130, Manchester, WA 98353 USA.
EM des.maynard@noaa.gov; joan.trial@maine.gov
NR 80
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U1 6
U2 37
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0960-3166
EI 1573-5184
J9 REV FISH BIOL FISHER
JI Rev. Fish. Biol. Fish.
PD SEP
PY 2014
VL 24
IS 3
SI SI
BP 803
EP 817
DI 10.1007/s11160-013-9341-7
PG 15
WC Fisheries; Marine & Freshwater Biology
SC Fisheries; Marine & Freshwater Biology
GA AN2ZS
UT WOS:000340455200008
ER
PT J
AU Trail, M
Tsimpidi, AP
Liu, P
Tsigaridis, K
Rudokas, J
Miller, P
Nenes, A
Hu, Y
Russell, AG
AF Trail, M.
Tsimpidi, A. P.
Liu, P.
Tsigaridis, K.
Rudokas, J.
Miller, P.
Nenes, A.
Hu, Y.
Russell, A. G.
TI Sensitivity of air quality to potential future climate change and
emissions in the United States and major cities
SO ATMOSPHERIC ENVIRONMENT
LA English
DT Article
DE Climate change; Air quality; Sensitivity; CMAQ; Downscaling; Projecting
emissions
ID US ANTHROPOGENIC AEROSOLS; MODEL; SCENARIOS; OZONE; GENERATION;
MORTALITY; BURDEN; HEALTH
AB Simulated present and future air quality is compared for the years 2006-2010 and 2048-2052 over the contiguous United States (CONUS) using the Community Multi-scale Air Quality (CMAQ) model. Regionally downscaled present and future climate results are developed using GISS and the Weather Research Forecasting (WRF) model. Present and future emissions are estimated using MARKAL 9R model. O-3 and PM2.5 sensitivities to precursor emissions for the years 2010 and 2050 are calculated using CMAQ-DDM (Direct Decoupled Method). We find major improvements in future U.S. air quality including generally decreased MDA8 (maximum daily 8-hr average O-3) mixing ratios and PM2.5 concentrations and reduced frequency of NAAQS O-3 standard exceedances in most major U.S. cities. The Eastern and Pacific U.S. experience the largest reductions in summertime seasonal average MDA8 (up to 12 ppb) with localized decreases in the 4th highest MDA8 of the year, decreasing by up to 25 ppb. Results from a Climate Penalty (CP) scenario isolate the impact of climate change on air quality and show that future climate change tends to increase O-3 mixing ratios in some regions of the U.S., with climate change causing increases of over 10 ppb in the annual 4th highest MDA8 in Los Angeles. Seasonal average PM2.5 decreases (2-4 mu g m(-3)) over the Eastern U.S. are accounted for by decreases in sulfate and nitrate concentrations resulting from reduced mobile and point source emissions of NOx and SOx. (C) 2014 Elsevier Ltd. All rights reserved.
C1 [Trail, M.; Tsimpidi, A. P.; Liu, P.; Hu, Y.; Russell, A. G.] Georgia Inst Technol, Sch Civil & Environm Engn, Atlanta, GA 30332 USA.
[Liu, P.; Nenes, A.] Georgia Inst Technol, Sch Chem & Biomol Engn, Atlanta, GA 30332 USA.
[Tsigaridis, K.] Columbia Univ, Ctr Climate Syst Res, New York, NY 10025 USA.
[Tsigaridis, K.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
[Rudokas, J.; Miller, P.] Northeast States Coordinated Air Use Management, Boston, MA 02111 USA.
[Nenes, A.] Georgia Inst Technol, Sch Earth & Atmospher Sci, Atlanta, GA 30332 USA.
RP Trail, M (reprint author), Georgia Inst Technol, Sch Civil & Environm Engn, Atlanta, GA 30332 USA.
EM mcus2rail@gmail.com
RI Hu, Yongtao/H-7543-2016
OI Hu, Yongtao/0000-0002-5161-0592
FU US EPA [EPA-G2008-STAR-J1]; NASA
FX While this work was supported, in part, by grants from the US EPA
(EPA-G2008-STAR-J1) and NASA, reference herein to any specific
commercial products, process, or service by trade name, trademark,
manufacturer, or otherwise, does not necessarily constitute or imply
their endorsement or recommendation. The views and opinions of authors
expressed herein are those of the authors and do not necessarily state
or reflect those of the United States Government.
NR 41
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U1 6
U2 69
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 1352-2310
EI 1873-2844
J9 ATMOS ENVIRON
JI Atmos. Environ.
PD SEP
PY 2014
VL 94
BP 552
EP 563
DI 10.1016/j.atmosenv.2014.05.079
PG 12
WC Environmental Sciences; Meteorology & Atmospheric Sciences
SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences
GA AN1AY
UT WOS:000340316300060
ER
PT J
AU Duncan, BN
Prados, AI
Lamsal, LN
Liu, Y
Streets, DG
Gupta, P
Hilsenrath, E
Kahn, RA
Nielsen, JE
Beyersdorf, AJ
Burton, SP
Fiore, AM
Fishman, J
Henze, DK
Hostetler, CA
Krotkov, NA
Lee, P
Lin, MY
Pawson, S
Pfister, G
Pickering, KE
Pierce, RB
Yoshida, Y
Ziemba, LD
AF Duncan, Bryan N.
Prados, Ana I.
Lamsal, Lok N.
Liu, Yang
Streets, David G.
Gupta, Pawan
Hilsenrath, Ernest
Kahn, Ralph A.
Nielsen, J. Eric
Beyersdorf, Andreas J.
Burton, Sharon P.
Fiore, Arlene M.
Fishman, Jack
Henze, Daven K.
Hostetler, Chris A.
Krotkov, Nickolay A.
Lee, Pius
Lin, Meiyun
Pawson, Steven
Pfister, Gabriele
Pickering, Kenneth E.
Pierce, R. Bradley
Yoshida, Yasuko
Ziemba, Luke D.
TI Satellite data of atmospheric pollution for US air quality applications:
Examples of applications, summary of data end-user resources, answers to
FAQs, and common mistakes to avoid
SO ATMOSPHERIC ENVIRONMENT
LA English
DT Review
DE Satellite data; Air quality; End-user resources; Remote sensing
ID AEROSOL OPTICAL DEPTH; OZONE MONITORING EXPERIMENT; RETRIEVAL ALGORITHM;
TROPOSPHERIC OZONE; ECONOMIC RECESSION; ISOPRENE EMISSIONS;
NITROGEN-OXIDES; UNITED-STATES; NOX EMISSIONS; MEXICO-CITY
AB Satellite data of atmospheric pollutants are becoming more widely used in the decision-making and environmental management activities of public, private sector and non-profit organizations. They are employed for estimating emissions, tracking pollutant plumes, supporting air quality forecasting activities, providing evidence for "exceptional event" declarations, monitoring regional long-term trends, and evaluating air quality model output. However, many air quality managers are not taking full advantage of the data for these applications nor has the full potential of satellite data for air quality applications been realized. A key barrier is the inherent difficulties associated with accessing, processing, and properly interpreting observational data. A degree of technical skill is required on the part of the data end-user, which is often problematic for air quality agencies with limited resources. Therefore, we 1) review the primary uses of satellite data for air quality applications, 2) provide some background information on satellite capabilities for measuring pollutants, 3) discuss the-many resources available to the end-user for accessing, processing, and visualizing the data, and 4) provide answers to common questions in plain language. Published by Elsevier Ltd.
C1 [Duncan, Bryan N.; Prados, Ana I.; Lamsal, Lok N.; Gupta, Pawan; Kahn, Ralph A.; Krotkov, Nickolay A.; Pawson, Steven; Pickering, Kenneth E.; Yoshida, Yasuko] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Prados, Ana I.; Hilsenrath, Ernest] Univ Maryland, Joint Ctr Earth Syst Technol, Baltimore, MD 21201 USA.
[Lamsal, Lok N.; Gupta, Pawan] Univ Space Res Assoc, Goddard Earth Sci Technol & Res, Columbia, MD USA.
[Liu, Yang] Emory Univ, Rollins Sch Publ Hlth, Atlanta, GA 30322 USA.
[Streets, David G.] Argonne Natl Lab, Argonne, IL 60439 USA.
[Hilsenrath, Ernest] Sigma Space Corp, Lanham, MD USA.
[Nielsen, J. Eric; Yoshida, Yasuko] Sci Syst & Applicat Inc, Lanham, MD USA.
[Beyersdorf, Andreas J.; Burton, Sharon P.; Hostetler, Chris A.; Ziemba, Luke D.] NASA, Langley Res Ctr, Hampton, VA 23665 USA.
[Fiore, Arlene M.] Columbia Univ, Dept Earth & Environm Sci, Palisades, NY USA.
[Fiore, Arlene M.] Columbia Univ, Lamont Doherty Earth Observ, Palisades, NY USA.
[Fishman, Jack] St Louis Univ, St Louis, MO 63103 USA.
[Henze, Daven K.] Univ Colorado, Boulder, CO 80309 USA.
[Lee, Pius] NOAA, College Pk, MD USA.
[Lin, Meiyun] Princeton Univ, Princeton, NJ 08544 USA.
[Lin, Meiyun] NOAA, Geophys Fluid Dynam Lab, Princeton, NJ USA.
[Pfister, Gabriele] Natl Ctr Atmospher Res, Boulder, CO 80307 USA.
[Pierce, R. Bradley] NOAA, Madison, WI USA.
RP Duncan, BN (reprint author), NASA, Goddard Space Flight Ctr, Code 614, Greenbelt, MD 20771 USA.
EM Bryan.N.Duncan@nasa.gov
RI Lin, Meiyun/D-6107-2013; Pierce, Robert Bradley/F-5609-2010; Krotkov,
Nickolay/E-1541-2012; Lee, Pius/D-5201-2016; Pickering,
Kenneth/E-6274-2012; Pawson, Steven/I-1865-2014; Duncan,
Bryan/A-5962-2011
OI Lin, Meiyun/0000-0003-3852-3491; Pierce, Robert
Bradley/0000-0002-2767-1643; Krotkov, Nickolay/0000-0001-6170-6750;
Pawson, Steven/0000-0003-0200-717X;
FU NASA Air Quality Applied Sciences Team (AQAST); Applied Remote SEnsing
Training (ARSET) program, within NASA's Applied Sciences Program
FX This work was funded by the NASA Air Quality Applied Sciences Team
(AQAST) and the Applied Remote SEnsing Training (ARSET) program, within
NASA's Applied Sciences Program. We thank Ginger Butcher, the NASA Aura
Mission's education and public outreach lead, for her comments which
greatly improved the readability of the article.
NR 89
TC 29
Z9 29
U1 4
U2 71
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 1352-2310
EI 1873-2844
J9 ATMOS ENVIRON
JI Atmos. Environ.
PD SEP
PY 2014
VL 94
BP 647
EP 662
DI 10.1016/j.atmosenv.2014.05.061
PG 16
WC Environmental Sciences; Meteorology & Atmospheric Sciences
SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences
GA AN1AY
UT WOS:000340316300069
ER
PT J
AU Stapleton, SE
Pineda, EJ
Gries, T
Waas, AM
AF Stapleton, Scott E.
Pineda, Evan J.
Gries, Thomas
Waas, Anthony M.
TI Adaptive shape functions and internal mesh adaptation for modeling
progressive failure in adhesively bonded joints
SO INTERNATIONAL JOURNAL OF SOLIDS AND STRUCTURES
LA English
DT Article
DE Adhesion; Bonded; Crack; Finite element; Joining; Numerical methods;
Adaptive shape functions; Adaptive mesh
ID COMPOSITE JOINTS; FINITE-ELEMENT; LAP JOINTS; ELASTIC-FOUNDATION;
STIFFNESS-MATRIX; ANALYSIS TOOLS; ORDER THEORY; BEAMS; CRITERION;
STRENGTH
AB Macroscopic finite elements are elements with an embedded analytical solution that can capture detailed local fields, enabling more efficient, mesh independent finite element analysis. The shape functions are determined based on the analytical model rather than prescribed. This method was applied to adhesively bonded joints to model joint behavior with one element through the thickness. This study demonstrates two methods of maintaining the fidelity of such elements during adhesive non-linearity and cracking without increasing the mesh needed for an accurate solution. The first method uses adaptive shape functions, where the shape functions are recalculated at each load step based on the softening of the adhesive. The second method is internal mesh adaption, where cracking of the adhesive within an element is captured by further discretizing the element internally to represent the partially cracked geometry. By keeping mesh adaptations within an element, a finer mesh can be used during the, analysis without affecting the global finite element model mesh. Examples are shown which highlight when each method is most effective in reducing the number of elements needed to capture adhesive nonlinearity and cracking. These methods are validated against analogous finite element models utilizing cohesive zone elements. (C) 2014 Elsevier Ltd. All rights reserved.
C1 [Stapleton, Scott E.; Gries, Thomas] Rhein Westfal TH Aachen, Inst Textile Technol, D-52074 Aachen, Germany.
[Pineda, Evan J.] NASA, Glenn Res Ctr, Struct & Mat Div, Cleveland, OH 44135 USA.
[Waas, Anthony M.] Univ Michigan, Dept Aerosp Engn, Ann Arbor, MI 48105 USA.
RP Stapleton, SE (reprint author), Rhein Westfal TH Aachen, Inst Textile Technol, D-52074 Aachen, Germany.
EM sstaple@umich.edu
FU Space Vehicle Technology Institute [NCC3-989]; NASA; U.S. Department of
Defense; NASA John H. Glenn Research Center at Lewis Field through the
NASA Graduate Student Researchers Project Fellowship
FX Portions of this work were financially supported by the Space Vehicle
Technology Institute under Grant No. NCC3-989, jointly funded by NASA
and the U.S. Department of Defense. The bulk of the financial support
was provided by NASA John H. Glenn Research Center at Lewis Field
through the NASA Graduate Student Researchers Project Fellowship.
NR 43
TC 2
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U1 2
U2 11
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0020-7683
EI 1879-2146
J9 INT J SOLIDS STRUCT
JI Int. J. Solids Struct.
PD SEP
PY 2014
VL 51
IS 18
BP 3252
EP 3264
DI 10.1016/j.ijsolstr.2014.05.022
PG 13
WC Mechanics
SC Mechanics
GA AM8QC
UT WOS:000340141100023
ER
PT J
AU Porst, JP
Bandler, SR
Adams, JS
Balvin, MA
Busch, SE
Eckart, ME
Kelley, RL
Kilbourne, CA
Lee, SJ
Nagler, PC
Porter, FS
Sadleir, JE
Seidel, GM
Smith, SJ
Stevenson, TR
AF Porst, J. -P.
Bandler, S. R.
Adams, J. S.
Balvin, M. A.
Busch, S. E.
Eckart, M. E.
Kelley, R. L.
Kilbourne, C. A.
Lee, S. J.
Nagler, P. C.
Porter, F. S.
Sadleir, J. E.
Seidel, G. M.
Smith, S. J.
Stevenson, T. R.
TI Characterization and Performance of Magnetic Calorimeters for
Applications in X-ray Spectroscopy
SO JOURNAL OF LOW TEMPERATURE PHYSICS
LA English
DT Article
DE Magnetic calorimeter; Microcalorimeter; X-ray; Spectrometer;
Multiplexing
ID HIGH-RESOLUTION
AB We have developed prototype arrays of metallic magnetic calorimeters for applications in X-ray astronomy. Each pixel consists of an all-gold X-ray absorber in good thermal contact to a gold-erbium paramagnetic thin film thermometer that is operated in the temperature range of 30-100 mK. The para-magnetic response is coupled to a SQUID amplifier. We have characterized pixels in an array and observed the expected temperature dependence of the magnetization and heat capacity. We have demonstrated a full width at half maximum energy resolution of 1.7 0.1 eV at 6 keV and have also read out these devices using time-division multiplexing.
C1 [Porst, J. -P.; Bandler, S. R.; Adams, J. S.; Balvin, M. A.; Busch, S. E.; Eckart, M. E.; Kelley, R. L.; Kilbourne, C. A.; Lee, S. J.; Nagler, P. C.; Porter, F. S.; Sadleir, J. E.; Smith, S. J.; Stevenson, T. R.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Porst, J. -P.] CRESST, Columbia, MD 21044 USA.
[Porst, J. -P.] USRA, Columbia, MD 21044 USA.
[Bandler, S. R.] CRESST, College Pk, MD 20742 USA.
[Bandler, S. R.] Univ Maryland, College Pk, MD 20742 USA.
[Adams, J. S.; Eckart, M. E.; Smith, S. J.] CRESST, Baltimore, MD 21250 USA.
[Adams, J. S.; Eckart, M. E.; Smith, S. J.] Univ Maryland Baltimore Cty, Baltimore, MD 21250 USA.
[Busch, S. E.; Lee, S. J.] NASA, Postdoctoral Program, Oakridge, TN USA.
[Nagler, P. C.; Seidel, G. M.] Brown Univ, Providence, RI 02912 USA.
RP Porst, JP (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
EM jpporst@gmail.com; Simon.R.Bandler@nasa.gov
RI Bandler, Simon/A-6258-2010; Smith, Stephen/B-1256-2008; Lee, Sang
Jun/A-3892-2015; Porter, Frederick/D-3501-2012
OI Bandler, Simon/0000-0002-5112-8106; Smith, Stephen/0000-0003-4096-4675;
Lee, Sang Jun/0000-0002-8199-3993; Porter, Frederick/0000-0002-6374-1119
FU NASA Office of Space Science ROSES program [NNX12AL50G]
FX We would like to thank J. Beyer of the Physikalisch-Technische
Bundesanstalt (PTB) in Berlin for providing the SQUIDs used in these
measurements and for many useful and stimulating discussions. We
gratefully acknowledge the financial support of NASA Office of Space
Science ROSES program, contract NNX12AL50G.
NR 10
TC 6
Z9 6
U1 0
U2 6
PU SPRINGER/PLENUM PUBLISHERS
PI NEW YORK
PA 233 SPRING ST, NEW YORK, NY 10013 USA
SN 0022-2291
EI 1573-7357
J9 J LOW TEMP PHYS
JI J. Low Temp. Phys.
PD SEP
PY 2014
VL 176
IS 5-6
BP 617
EP 623
DI 10.1007/s10909-013-1019-y
PG 7
WC Physics, Applied; Physics, Condensed Matter
SC Physics
GA AM5DE
UT WOS:000339875400001
ER
PT J
AU Shirokoff, E
Barry, PS
Bradford, CM
Chattopadhyay, G
Day, P
Doyle, S
Hailey-Dunsheath, S
Hollister, MI
Kovacs, A
Leduc, HG
McKenney, CM
Mauskopf, P
Nguyen, HT
O'Brient, R
Padin, S
Reck, TJ
Swenson, LJ
Tucker, CE
Zmuidzinas, J
AF Shirokoff, E.
Barry, P. S.
Bradford, C. M.
Chattopadhyay, G.
Day, P.
Doyle, S.
Hailey-Dunsheath, S.
Hollister, M. I.
Kovacs, A.
Leduc, H. G.
McKenney, C. M.
Mauskopf, P.
Nguyen, H. T.
O'Brient, R.
Padin, S.
Reck, T. J.
Swenson, L. J.
Tucker, C. E.
Zmuidzinas, J.
TI Design and Performance of SuperSpec: An On-Chip, KID-Based,
mm-Wavelength Spectrometer
SO JOURNAL OF LOW TEMPERATURE PHYSICS
LA English
DT Article
DE Kinetic inductance detectors; Resonators; Millimeter-wavelength;
Spectroscopy
ID ASTRONOMY
AB SuperSpec is an ultra-compact spectrometer-on-a-chip for mm and submm wavelength astronomy. Its very small size, wide spectral bandwidth, and highly multiplexed detector readout will enable construction of powerful multi-object spectrometers for observations of galaxies at high redshift. SuperSpec is a filter bank with planar, lithographed, superconducting transmission line resonator filters and lumped-element kinetic inductance detectors made from Titanium Nitride. We have built an 81 detector prototype that operates in the 195-310 GHz band. The prototype has a wide-band metal feed horn with a transition to microstrip that feeds the filter bank. The prototype has demonstrated optical filter bank channels with a range of resolving powers from 300 to 700, measured fractional frequency noise of at Hz.
C1 [Shirokoff, E.; Hailey-Dunsheath, S.; Hollister, M. I.; Kovacs, A.; McKenney, C. M.; O'Brient, R.; Padin, S.; Zmuidzinas, J.] CALTECH, Pasadena, CA 91125 USA.
[Barry, P. S.; Doyle, S.; Mauskopf, P.; Tucker, C. E.] Cardiff Univ, Sch Phys & Astron, Cardiff CF10 3AX, S Glam, Wales.
[Bradford, C. M.; Chattopadhyay, G.; Day, P.; Leduc, H. G.; Nguyen, H. T.; O'Brient, R.; Reck, T. J.; Swenson, L. J.; Zmuidzinas, J.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Mauskopf, P.] Arizona State Univ, Tempe, AZ USA.
RP Shirokoff, E (reprint author), CALTECH, Pasadena, CA 91125 USA.
EM erik.shirokoff@caltech.edu
RI Kovacs, Attila/C-1171-2010
OI Kovacs, Attila/0000-0001-8991-9088
FU NASA Astrophysics Research and Analysis (APRA) [399131.02.06.03.43]; W.
M. Keck Institute; NASA; Science and Technology Facilities Council
[ST/G002711/1, ST/J001449/1]
FX This project is supported by NASA Astrophysics Research and Analysis
(APRA) Grant No. 399131.02.06.03.43. ES, CMM, and LJS acknowledge
support from the W. M. Keck Institute for Space Studies. MIH, LJS, and
TR acknowledge support from the NASA Postdoctoral Program. PSB
acknowledges the continuing support from the Science and Technology
Facilities Council Ph.D. studentship programme and grant programmes
ST/G002711/1 and ST/J001449/1. Device fabrication was performed the JPL
Microdevices Laboratory.
NR 14
TC 5
Z9 5
U1 1
U2 6
PU SPRINGER/PLENUM PUBLISHERS
PI NEW YORK
PA 233 SPRING ST, NEW YORK, NY 10013 USA
SN 0022-2291
EI 1573-7357
J9 J LOW TEMP PHYS
JI J. Low Temp. Phys.
PD SEP
PY 2014
VL 176
IS 5-6
BP 657
EP 662
DI 10.1007/s10909-014-1122-8
PG 6
WC Physics, Applied; Physics, Condensed Matter
SC Physics
GA AM5DE
UT WOS:000339875400007
ER
PT J
AU Datta, R
Hubmayr, J
Munson, C
Austermann, J
Beall, J
Becker, D
Cho, HM
Halverson, N
Hilton, G
Irwin, K
Li, D
McMahon, J
Newburgh, L
Nibarger, J
Niemack, M
Schmitt, B
Smith, H
Staggs, S
Van Lanen, J
Wollack, E
AF Datta, R.
Hubmayr, J.
Munson, C.
Austermann, J.
Beall, J.
Becker, D.
Cho, H. M.
Halverson, N.
Hilton, G.
Irwin, K.
Li, D.
McMahon, J.
Newburgh, L.
Nibarger, J.
Niemack, M.
Schmitt, B.
Smith, H.
Staggs, S.
Van Lanen, J.
Wollack, E.
TI Horn Coupled Multichroic Polarimeters for the Atacama Cosmology
Telescope Polarization Experiment
SO JOURNAL OF LOW TEMPERATURE PHYSICS
LA English
DT Article
DE Cosmic microwave background; Superconducting detectors; Feedhorn; TES;
Polarimeter; Millimeter-wave; Silicon lenses; Antireflection coating
AB Multichroic polarization sensitive detectors enable increased sensitivity and spectral coverage for observations of the cosmic microwave background. An array optimized for dual frequency detectors can provide 1.7 times gain in sensitivity compared to a single frequency array. We present the design and measurements of horn coupled multichroic polarimeters encompassing the 90 and 150 GHz frequency bands and discuss our plans to field an array of these detectors as part of the ACTPol project.
C1 [Datta, R.; Munson, C.; McMahon, J.; Smith, H.] Univ Michigan, Dept Phys, Ann Arbor, MI 48109 USA.
[Hubmayr, J.; Beall, J.; Becker, D.; Cho, H. M.; Hilton, G.; Irwin, K.; Li, D.; Niemack, M.; Van Lanen, J.] NIST, Boulder, CO 80305 USA.
[Austermann, J.; Halverson, N.] Univ Colorado, Dept Astrophys Sci, Boulder, CO 80309 USA.
[Newburgh, L.; Staggs, S.] Princeton Univ, Dept Phys, Princeton, NJ 08544 USA.
[Nibarger, J.] NIST, Boulder Microfabricat Facil, Boulder, CO 80305 USA.
[Niemack, M.] Cornell Univ, Dept Phys, Ithaca, NY 14853 USA.
[Schmitt, B.] Univ Penn, Dept Phys & Astron, Philadelphia, PA 19104 USA.
[Wollack, E.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Datta, R (reprint author), Univ Michigan, Dept Phys, Ann Arbor, MI 48109 USA.
EM dattar@umich.edu
RI Wollack, Edward/D-4467-2012
OI Wollack, Edward/0000-0002-7567-4451
FU NASA [NNX13AE56G]; NASA Space Technology Research Fellowship
[NNX12AM32H]; U.S. National Science Foundation [AST-0965625,
PHY-1214379]
FX This work was supported by NASA through award NNX13AE56G and the NASA
Space Technology Research Fellowship grant NNX12AM32H and by the U.S.
National Science Foundation through awards AST-0965625 and PHY-1214379.
NR 9
TC 14
Z9 14
U1 0
U2 7
PU SPRINGER/PLENUM PUBLISHERS
PI NEW YORK
PA 233 SPRING ST, NEW YORK, NY 10013 USA
SN 0022-2291
EI 1573-7357
J9 J LOW TEMP PHYS
JI J. Low Temp. Phys.
PD SEP
PY 2014
VL 176
IS 5-6
BP 670
EP 676
DI 10.1007/s10909-014-1134-4
PG 7
WC Physics, Applied; Physics, Condensed Matter
SC Physics
GA AM5DE
UT WOS:000339875400009
ER
PT J
AU Grace, EA
Beall, J
Cho, HM
Devlin, MJ
Fox, A
Hilton, G
Hubmayr, J
Irwin, K
Klein, J
Li, D
Lungu, M
Newburgh, LB
Nibarger, J
Niemack, MD
McMahon, J
Page, LA
Pappas, C
Schmitt, BL
Staggs, ST
Van Lanen, J
Wollack, E
AF Grace, E. A.
Beall, J.
Cho, H. M.
Devlin, M. J.
Fox, A.
Hilton, G.
Hubmayr, J.
Irwin, K.
Klein, J.
Li, D.
Lungu, M.
Newburgh, L. B.
Nibarger, J.
Niemack, M. D.
McMahon, J.
Page, L. A.
Pappas, C.
Schmitt, B. L.
Staggs, S. T.
Van Lanen, J.
Wollack, E.
TI Characterization and Performance of a Kilo-TES Sub-Array for ACTPol
SO JOURNAL OF LOW TEMPERATURE PHYSICS
LA English
DT Article
DE Cosmic microwave background; Transition edge sensor; Bolometer;
Polarimetry
AB ACTPol is a polarization-sensitive receiver upgrade to the Atacama Cosmology Telescope (ACT) which will make millimeter wavelength measurements of the small-scale polarization anisotropies of the cosmic microwave background to investigate the properties of inflation, dark energy, dark matter, and neutrinos in the early Universe. ACTPol will employ three arrays of transition edge sensor (TES) bolometer detectors. The detectors, with a target transition temperature of 150 mK, will be operated at a bath temperature of 100 mK provided by a dilution refrigerator. One array operating at a central frequency of 150 GHz and consisting of 1024 TESes achieved first light at the ACT site in July 2013. We anticipate fielding the remainder of the focal plane, consisting of a second 150 GHz array and a multi-chroic array sensitive to 90 and 150 GHz, at the end of the 2013 observing season. In these proceedings, we present characterization of key detector parameters from measurements performed on the first array both in the lab and during initial field testing. We comment on the design goals, measurements, and uniformity of the detector transition temperatures, saturation powers, and thermal conductivities while detailing measurement methods and results for the detector optical efficiencies and time constants.
C1 [Grace, E. A.; Page, L. A.; Pappas, C.; Staggs, S. T.] Princeton Univ, Dept Phys, Princeton, NJ 08540 USA.
[Beall, J.; Cho, H. M.; Fox, A.; Hilton, G.; Hubmayr, J.; Irwin, K.; Li, D.; Nibarger, J.; Van Lanen, J.] NIST, Boulder, CO 80305 USA.
[Devlin, M. J.; Klein, J.; Lungu, M.; Schmitt, B. L.] Univ Penn, Dept Phys, Philadelphia, PA 19104 USA.
[Newburgh, L. B.] Univ Toronto, Dunlap Inst, Toronto, ON M5S 3H4, Canada.
[Niemack, M. D.] Cornell Univ, Dept Phys, Ithaca, NY 14853 USA.
[McMahon, J.] Univ Michigan, Ann Arbor, MI 48109 USA.
[Wollack, E.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Grace, EA (reprint author), Princeton Univ, Dept Phys, Princeton, NJ 08540 USA.
EM egrace@princeton.edu
RI Wollack, Edward/D-4467-2012
OI Wollack, Edward/0000-0002-7567-4451
FU U.S. National Science Foundation [AST-0965625, PHY-0855887,
PHY-1214379]; NIST Quantum Initiative; NASA Office of the Chief
Technologists Space Technology Research Fellowship awards
FX This work was supported by the U.S. National Science Foundation through
awards AST-0965625, PHY-0855887 and PHY-1214379. The NIST authors would
like to acknowledge the support of the NIST Quantum Initiative. The work
of E.A. Grace and B. Schmitt were supported by NASA Office of the Chief
Technologists Space Technology Research Fellowship awards. We would like
to acknowledge the work of Bert Harrop in the bonding and assembly of
the first array.
NR 10
TC 2
Z9 2
U1 0
U2 5
PU SPRINGER/PLENUM PUBLISHERS
PI NEW YORK
PA 233 SPRING ST, NEW YORK, NY 10013 USA
SN 0022-2291
EI 1573-7357
J9 J LOW TEMP PHYS
JI J. Low Temp. Phys.
PD SEP
PY 2014
VL 176
IS 5-6
BP 705
EP 711
DI 10.1007/s10909-014-1125-5
PG 7
WC Physics, Applied; Physics, Condensed Matter
SC Physics
GA AM5DE
UT WOS:000339875400014
ER
PT J
AU Barron, D
Ade, P
Anthony, A
Arnold, K
Boettger, D
Borrill, J
Chapman, S
Chinone, Y
Dobbs, M
Edwards, J
Errard, J
Fabbian, G
Flanigan, D
Fuller, G
Ghribi, A
Grainger, W
Halverson, N
Hasegawa, M
Hattori, K
Hazumi, M
Holzapfel, W
Howard, J
Hyland, P
Jaehnig, G
Jaffe, A
Keating, B
Kermish, Z
Keskitalo, R
Kisner, T
Lee, AT
Le Jeune, M
Linder, E
Lungu, M
Matsuda, F
Matsumura, T
Meng, X
Miller, NJ
Morii, H
Moyerman, S
Myers, M
Nishino, H
Paar, H
Peloton, J
Quealy, E
Rebeiz, G
Reichardt, CL
Richards, PL
Ross, C
Shimizu, A
Shimmin, C
Shimon, M
Sholl, M
Siritanasak, P
Spieler, H
Stebor, N
Steinbach, B
Stompor, R
Suzuki, A
Tomaru, T
Tucker, C
Yadav, A
Zahn, O
AF Barron, D.
Ade, P.
Anthony, A.
Arnold, K.
Boettger, D.
Borrill, J.
Chapman, S.
Chinone, Y.
Dobbs, M.
Edwards, J.
Errard, J.
Fabbian, G.
Flanigan, D.
Fuller, G.
Ghribi, A.
Grainger, W.
Halverson, N.
Hasegawa, M.
Hattori, K.
Hazumi, M.
Holzapfel, W.
Howard, J.
Hyland, P.
Jaehnig, G.
Jaffe, A.
Keating, B.
Kermish, Z.
Keskitalo, R.
Kisner, T.
Lee, A. T.
Le Jeune, M.
Linder, E.
Lungu, M.
Matsuda, F.
Matsumura, T.
Meng, X.
Miller, N. J.
Morii, H.
Moyerman, S.
Myers, M.
Nishino, H.
Paar, H.
Peloton, J.
Quealy, E.
Rebeiz, G.
Reichardt, C. L.
Richards, P. L.
Ross, C.
Shimizu, A.
Shimmin, C.
Shimon, M.
Sholl, M.
Siritanasak, P.
Spieler, H.
Stebor, N.
Steinbach, B.
Stompor, R.
Suzuki, A.
Tomaru, T.
Tucker, C.
Yadav, A.
Zahn, O.
TI The POLARBEAR Cosmic Microwave Background Polarization Experiment
SO JOURNAL OF LOW TEMPERATURE PHYSICS
LA English
DT Article
DE Cosmic microwave background; CMB polarization; Millimeter-wave
AB The polarbear cosmic microwave background (CMB) polarization experiment has been observing since early 2012 from its 5,200 m site in the Atacama Desert in Northern Chile. polarbear's measurements will characterize the expected CMB polarization due to gravitational lensing by large scale structure, and search for the possible B-mode polarization signature of inflationary gravitational waves. polarbear's 250 mK focal plane detector array consists of 1,274 polarization-sensitive antenna-coupled bolometers, each with an associated lithographed band-defining filter and contacting dielectric lenslet, an architecture unique in current CMB experiments. The status of the polarbear instrument, its focal plane, and the analysis of its measurements are presented.
C1 [Barron, D.; Arnold, K.; Boettger, D.; Edwards, J.; Fuller, G.; Keating, B.; Matsuda, F.; Meng, X.; Moyerman, S.; Paar, H.; Rebeiz, G.; Siritanasak, P.; Stebor, N.; Yadav, A.] Univ Calif San Diego, Dept Phys, La Jolla, CA 92093 USA.
[Ade, P.; Tucker, C.] Cardiff Univ, Sch Phys & Astron, Cardiff CF10 3AX, S Glam, Wales.
[Anthony, A.; Halverson, N.; Jaehnig, G.] Univ Colorado, Dept Astrophys & Planetary Sci, Boulder, CO 80309 USA.
[Borrill, J.; Errard, J.; Keskitalo, R.; Kisner, T.] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Computat Cosmol Ctr, Berkeley, CA 94720 USA.
[Borrill, J.; Richards, P. L.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
[Chapman, S.; Ross, C.] Dalhousie Univ, Dept Phys, Halifax, NS B3H 3J5, Canada.
[Chinone, Y.; Hasegawa, M.; Hattori, K.; Hazumi, M.; Matsumura, T.; Morii, H.; Shimizu, A.; Tomaru, T.] High Energy Accelerator Res Org KEK, Tsukuba, Ibaraki, Japan.
[Dobbs, M.] McGill Univ, Dept Phys, Montreal, PQ, Canada.
[Fabbian, G.; Le Jeune, M.; Peloton, J.; Stompor, R.] Univ Paris 07, Lab Astroparticule & Cosmol APC, Paris, France.
[Flanigan, D.; Ghribi, A.; Holzapfel, W.; Howard, J.; Lee, A. T.; Lungu, M.; Myers, M.; Quealy, E.; Reichardt, C. L.; Richards, P. L.; Shimmin, C.; Steinbach, B.; Suzuki, A.] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA.
[Grainger, W.] STFC, Rutherford Appleton Lab, Didcot, Oxon, England.
[Hyland, P.] Austin Coll, Dept Phys, Sherman, TX 75090 USA.
[Jaffe, A.] Univ London Imperial Coll Sci Technol & Med, Dept Phys, London, England.
[Kermish, Z.] Princeton Univ, Princeton, NJ 08544 USA.
[Linder, E.; Sholl, M.; Spieler, H.; Zahn, O.] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Div Phys, Berkeley, CA 94720 USA.
[Miller, N. J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Nishino, H.] Univ Tokyo, Kavli Inst Phys & Math Universe, Kashiwa, Chiba, Japan.
[Shimon, M.] Tel Aviv Univ, IL-69978 Tel Aviv, Israel.
[Zahn, O.] Univ Calif Berkeley, Berkeley Ctr Cosmol Phys BCCP, Berkeley, CA 94720 USA.
RP Barron, D (reprint author), Univ Calif San Diego, Dept Phys, La Jolla, CA 92093 USA.
EM dbarron@physics.ucsd.edu
RI Holzapfel, William/I-4836-2015;
OI Fabbian, Giulio/0000-0002-3255-4695; Reichardt,
Christian/0000-0003-2226-9169
FU National Science Foundation [AST-0618398]; NASA [NNG06GJ08G]; Natural
Sciences and Engineering Research Council; Canadian Institute for
Advanced Research; MEXT KAKENHI [21111002]; Simons Foundation
FX POLARBEAR is funded by the National Science Foundation under Grant
AST-0618398. Antenna-coupled bolometer development at Berkeley is funded
by NASA under Grant NNG06GJ08G. The McGill authors acknowledge funding
from the Natural Sciences and Engineering Research Council and Canadian
Institute for Advanced Research. The KEK authors are supported by MEXT
KAKENHI Grant Number 21111002. The Chilean site is located in the Parque
Astronomico Atacama in agreement with the Comision Nacional de
Investigacion Cientifica y Tecnologica de Chile. The Simons Array is
funded by the Simons Foundation.
NR 14
TC 0
Z9 0
U1 3
U2 5
PU SPRINGER/PLENUM PUBLISHERS
PI NEW YORK
PA 233 SPRING ST, NEW YORK, NY 10013 USA
SN 0022-2291
EI 1573-7357
J9 J LOW TEMP PHYS
JI J. Low Temp. Phys.
PD SEP
PY 2014
VL 176
IS 5-6
BP 726
EP 732
DI 10.1007/s10909-013-1065-5
PG 7
WC Physics, Applied; Physics, Condensed Matter
SC Physics
GA AM5DE
UT WOS:000339875400017
ER
PT J
AU Johnson, BR
Ade, PAR
Araujo, D
Bradford, KJ
Chapman, D
Day, PK
Didier, J
Doyle, S
Eriksen, HK
Flanigan, D
Groppi, C
Hillbrand, S
Jones, G
Limon, M
Mauskopf, P
McCarrick, H
Miller, A
Mroczkowski, T
Reichborn-Kjennerud, B
Smiley, B
Sobrin, J
Wehus, IK
Zmuidzinas, J
AF Johnson, B. R.
Ade, P. A. R.
Araujo, D.
Bradford, K. J.
Chapman, D.
Day, P. K.
Didier, J.
Doyle, S.
Eriksen, H. K.
Flanigan, D.
Groppi, C.
Hillbrand, S.
Jones, G.
Limon, M.
Mauskopf, P.
McCarrick, H.
Miller, A.
Mroczkowski, T.
Reichborn-Kjennerud, B.
Smiley, B.
Sobrin, J.
Wehus, I. K.
Zmuidzinas, J.
TI The Detector System for the Stratospheric Kinetic Inductance Polarimeter
(SKIP)
SO JOURNAL OF LOW TEMPERATURE PHYSICS
LA English
DT Article
DE CMB; CIB; MKID; LEKID
AB The stratospheric kinetic inductance polarimeter is a proposed balloon-borne experiment designed to study the cosmic microwave background, the cosmic infrared background and Galactic dust emission by observing 1,133 deg of sky in the Northern Hemisphere with launches from Kiruna, Sweden. The instrument contains 2,317 single-polarization, horn-coupled, aluminum lumped-element kinetic inductance detectors (Lekids). The Lekids will be maintained at 100 mK with an adiabatic demagnetization refrigerator. The polarimeter operates in two configurations, one sensitive to a spectral band centered on 150 GHz and the other sensitive to 260 and 350 GHz bands. The detector readout system is based on the ROACH-1 board, and the detectors will be biased below 300 MHz. The detector array is fed by an F/2.4 crossed-Dragone telescope with a 500 mm aperture yielding a 15 arcmin FWHM beam at 150 GHz. To minimize detector loading and maximize sensitivity, the entire optical system will be cooled to 1 K. Linearly polarized sky signals will be modulated with a metal-mesh half-wave plate that is mounted at the telescope aperture and rotated by a superconducting magnetic bearing. The observation program consists of at least two, 5-day flights beginning with the 150 GHz observations.
C1 [Johnson, B. R.; Araujo, D.; Bradford, K. J.; Chapman, D.; Didier, J.; Flanigan, D.; Hillbrand, S.; Jones, G.; Limon, M.; McCarrick, H.; Miller, A.; Reichborn-Kjennerud, B.; Smiley, B.; Sobrin, J.] Columbia Univ, Dept Phys, New York, NY 10027 USA.
[Groppi, C.; Mauskopf, P.] Arizona State Univ, Dept Phys, Tempe, AZ 85287 USA.
[Mroczkowski, T.; Zmuidzinas, J.] CALTECH, Dept Phys, Pasadena, CA 91125 USA.
[Ade, P. A. R.; Doyle, S.] Cardiff Univ, Sch Phys & Astron, Cardiff CF243YB, S Glam, Wales.
[Eriksen, H. K.] Univ Oslo, Inst Theoret Astrophys, N-0315 Oslo, Norway.
[Jones, G.] Natl Radio Astron Observ, Charlottesville, VA 22903 USA.
[Day, P. K.; Wehus, I. K.; Zmuidzinas, J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Johnson, BR (reprint author), Columbia Univ, Dept Phys, 538 W 120th St, New York, NY 10027 USA.
EM bjohnson@phys.columbia.edu
OI Limon, Michele/0000-0002-5900-2698; Mroczkowski,
Tony/0000-0003-3816-5372
NR 12
TC 2
Z9 2
U1 1
U2 9
PU SPRINGER/PLENUM PUBLISHERS
PI NEW YORK
PA 233 SPRING ST, NEW YORK, NY 10013 USA
SN 0022-2291
EI 1573-7357
J9 J LOW TEMP PHYS
JI J. Low Temp. Phys.
PD SEP
PY 2014
VL 176
IS 5-6
BP 741
EP 748
DI 10.1007/s10909-013-1014-3
PG 8
WC Physics, Applied; Physics, Condensed Matter
SC Physics
GA AM5DE
UT WOS:000339875400019
ER
PT J
AU Pappas, CG
Beall, J
Brevick, J
Cho, HM
Devlin, MJ
Fox, A
Grace, EA
Hilton, GC
Hubmayr, J
Irwin, KD
Klein, J
Li, D
Lungu, M
Newburgh, LB
Nibarger, JP
Niemack, MD
McMahon, JJ
Page, LA
Schmitt, BL
Staggs, ST
Van Lanen, J
Wollack, EJ
AF Pappas, C. G.
Beall, J.
Brevick, J.
Cho, H. M.
Devlin, M. J.
Fox, A.
Grace, E. A.
Hilton, G. C.
Hubmayr, J.
Irwin, K. D.
Klein, J.
Li, D.
Lungu, M.
Newburgh, L. B.
Nibarger, J. P.
Niemack, M. D.
McMahon, J. J.
Page, L. A.
Schmitt, B. L.
Staggs, S. T.
Van Lanen, J.
Wollack, E. J.
TI Optical Efficiency and R(T,I) Measurements of ACTPol TESes Using Time
Domain Multiplexing Electronics
SO JOURNAL OF LOW TEMPERATURE PHYSICS
LA English
DT Article
DE Transition edge sensor (TES); Cosmic microwave background (CMB);
Polarization; Atacama cosmology telescope; ACTPol
ID TRANSITION-EDGE SENSORS
AB We present new data on feedhorn-coupled transition-edge sensor devices fabricated for the second-generation receiver (ACTPol) for the Atacama cosmology telescope (ACT). First, we describe optical efficiency measurements of the latest ACTPol detector wafer, which has a average optical efficiency. Next, we discuss measurements of the TES resistance as a function of temperature and bias current () using the ACTPol time-domain multiplexing electronics. Qualitative agreement between data at low bias current and the two-fluid model prediction is shown. Using the two-fluid model and low bias current data, and at our operating bias current are calculated.
C1 [Pappas, C. G.; Grace, E. A.; Page, L. A.; Staggs, S. T.] Princeton Univ, Dept Phys, Princeton, NJ 08544 USA.
[Niemack, M. D.] Cornell Univ, Dept Phys, Ithaca, NY 14853 USA.
[Wollack, E. J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[McMahon, J. J.] Univ Michigan, Dept Phys, Randall Lab 1440, Ann Arbor, MI 48109 USA.
[Beall, J.; Brevick, J.; Cho, H. M.; Fox, A.; Hilton, G. C.; Hubmayr, J.; Irwin, K. D.; Li, D.; Nibarger, J. P.; Van Lanen, J.] NIST, Quantum Elect & Photon Div, Boulder, CO 80305 USA.
[Devlin, M. J.; Klein, J.; Lungu, M.; Schmitt, B. L.] Univ Penn, Dept Phys & Astron, Philadelphia, PA 19104 USA.
[Newburgh, L. B.] Univ Toronto, Dept Astron & Astrophys, Toronto, ON M5S 3H4, Canada.
RP Pappas, CG (reprint author), Princeton Univ, Dept Phys, Jadwin Hall, Princeton, NJ 08544 USA.
EM cpappas@princeton.edu
RI Wollack, Edward/D-4467-2012
OI Wollack, Edward/0000-0002-7567-4451
NR 15
TC 1
Z9 1
U1 1
U2 5
PU SPRINGER/PLENUM PUBLISHERS
PI NEW YORK
PA 233 SPRING ST, NEW YORK, NY 10013 USA
SN 0022-2291
EI 1573-7357
J9 J LOW TEMP PHYS
JI J. Low Temp. Phys.
PD SEP
PY 2014
VL 176
IS 5-6
BP 749
EP 754
DI 10.1007/s10909-013-1066-4
PG 6
WC Physics, Applied; Physics, Condensed Matter
SC Physics
GA AM5DE
UT WOS:000339875400020
ER
PT J
AU Catalano, A
Ade, P
Atik, Y
Benoit, A
Breele, E
Bock, J
Camus, P
Charra, M
Crill, BP
Coron, N
Coulais, A
Desert, FX
Fauvet, L
Giraud-Heraud, Y
Guillaudin, O
Holmes, W
Jones, WC
Lamarre, JM
Macias-Perez, J
Martinez, M
Miniussi, A
Monfardini, A
Pajot, F
Patanchon, G
Pelissier, A
Piat, M
Puget, JL
Renault, C
Rosset, C
Santos, D
Sauve, A
Spencer, L
Sudiwala, R
AF Catalano, A.
Ade, P.
Atik, Y.
Benoit, A.
Breele, E.
Bock, J. J.
Camus, P.
Charra, M.
Crill, B. P.
Coron, N.
Coulais, A.
Desert, F. -X.
Fauvet, L.
Giraud-Heraud, Y.
Guillaudin, O.
Holmes, W.
Jones, W. C.
Lamarre, J. -M.
Macias-Perez, J.
Martinez, M.
Miniussi, A.
Monfardini, A.
Pajot, F.
Patanchon, G.
Pelissier, A.
Piat, M.
Puget, J. -L.
Renault, C.
Rosset, C.
Santos, D.
Sauve, A.
Spencer, L.
Sudiwala, R.
TI Characterization and Physical Explanation of Energetic Particles on
Planck HFI Instrument
SO JOURNAL OF LOW TEMPERATURE PHYSICS
LA English
DT Article
DE Planck satellite; High impedance bolometers; Cosmic rays
AB The Planck High Frequency Instrument (HFI) has been surveying the sky continuously from the second Lagrangian point (L2) between August 2009 and January 2012. It operates with 52 high impedance bolometers cooled at 100 mK in a range of frequency between 100 GHz and 1 THz with unprecedented sensitivity, but strong coupling with cosmic radiation. At L2, the particle flux is about 5 and is dominated by protons incident on the spacecraft. Protons with an energy above 40 MeV can penetrate the focal plane unit box causing two different effects: glitches in the raw data from direct interaction of cosmic rays with detectors (producing a data loss of about 15 % at the end of the mission) and thermal drifts in the bolometer plate at 100 mK adding non-Gaussian noise at frequencies below 0.1 Hz. The HFI consortium has made strong efforts in order to correct for this effect on the time ordered data and final Planck maps. This work intends to give a view of the physical explanation of the glitches observed in the HFI instrument in-flight. To reach this goal, we performed several ground-based experiments using protons and particles to test the impact of particles on the HFI spare bolometers with a better control of the environmental conditions with respect to the in-flight data. We have shown that the dominant part of glitches observed in the data comes from the impact of cosmic rays in the silicon die frame supporting the micro-machined bolometric detectors propagating energy mainly by ballistic phonons and by thermal diffusion. The implications of these results for future satellite missions will be discussed.
C1 [Catalano, A.; Guillaudin, O.; Macias-Perez, J.; Pelissier, A.; Renault, C.; Santos, D.] Univ Grenoble 1, Inst Natl Polytech Grenoble, Lab Phys Subatom & Cosmol, CNRS,IN2P3, F-38026 Grenoble, France.
[Ade, P.; Spencer, L.; Sudiwala, R.] Cardiff Univ, Sch Phys & Astron, Cardiff CF24 3AA, S Glam, Wales.
[Atik, Y.; Charra, M.; Coron, N.; Martinez, M.; Miniussi, A.; Pajot, F.; Puget, J. -L.] Univ Paris 11, CNRS, UMR8617, Inst Astrophys Spatiale, F-91405 Orsay, France.
[Benoit, A.; Camus, P.; Monfardini, A.] Univ Grenoble 1, CNRS, Inst Neel, F-38026 Grenoble, France.
[Breele, E.; Giraud-Heraud, Y.; Patanchon, G.; Piat, M.; Rosset, C.] Univ Paris 07, CNRS, UMR 7164, Paris, France.
[Bock, J. J.] CALTECH, Pasadena, CA 91125 USA.
[Bock, J. J.; Crill, B. P.; Holmes, W.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Coulais, A.; Lamarre, J. -M.] Observ Paris, CNRS, LERMA, F-75014 Paris, France.
[Desert, F. -X.] Univ Grenoble 1, IPAG, Grenoble CNRS INSU 1, UMR 5274, F-38041 Grenoble, France.
[Fauvet, L.] European Space Agcy, Estec, NL-2201 AZ Noordwijk, Netherlands.
[Jones, W. C.] Princeton Univ, Dept Phys, Princeton, NJ 08544 USA.
[Sauve, A.] IRAP, CNRS, F-31028 Toulouse 4, France.
RP Catalano, A (reprint author), Univ Grenoble 1, Inst Natl Polytech Grenoble, Lab Phys Subatom & Cosmol, CNRS,IN2P3, 53 Rue Martyrs, F-38026 Grenoble, France.
EM catalano@lpsc.in2p3.fr
RI Martinez, Maria/K-4827-2012
OI Martinez, Maria/0000-0002-9043-4691
NR 11
TC 4
Z9 4
U1 0
U2 7
PU SPRINGER/PLENUM PUBLISHERS
PI NEW YORK
PA 233 SPRING ST, NEW YORK, NY 10013 USA
SN 0022-2291
EI 1573-7357
J9 J LOW TEMP PHYS
JI J. Low Temp. Phys.
PD SEP
PY 2014
VL 176
IS 5-6
BP 773
EP 786
DI 10.1007/s10909-014-1116-6
PG 14
WC Physics, Applied; Physics, Condensed Matter
SC Physics
GA AM5DE
UT WOS:000339875400024
ER
PT J
AU Miniussi, A
Puget, JL
Holmes, W
Patanchon, G
Catalano, A
Giraud-Heraud, Y
Pajot, F
Piat, M
Vibert, L
AF Miniussi, A.
Puget, J. -L.
Holmes, W.
Patanchon, G.
Catalano, A.
Giraud-Heraud, Y.
Pajot, F.
Piat, M.
Vibert, L.
TI Study of Cosmic Ray Impact on Planck/HFI Low Temperature Detectors
SO JOURNAL OF LOW TEMPERATURE PHYSICS
LA English
DT Article
DE Cosmic ray; Particle; HFI; Planck; Bolometer
AB Once that the focal plane of the HFI instrument of the Planck mission (launched in May 2009) has reached operational temperature, we have observed the thermal effect of cosmic ray interaction with the Planck satellite, located at Lagrangian point L2. When a particle hits a component of the bolometers (e.g.: thermometer, grid or wafer) composing the focal plane of HFI, a thermal spike (called glitch), due to deposited energy, is observed. Processing these data revealed another effect due to high energy cosmic ray particle showers: High Coincidence Events (HCE), composed of glitches occurring coincidentally in many detectors and with a temperature increase from nK to K after the shower. A flux of about 100 HCE per hour has been calculated. Two types of HCE have been detected: fast and slow. For the first type, the untouched bolometers reach the same temperature as the touched ones in a few seconds which can be explained by a storage of the deposited energy in the stainless steel focal plane. The second type of HCE is not fully understood yet. These effects might be explained by extra conduction from the helium released from cryogenic surfaces, creating a temporary thermal link between the different stages of the HFI.
C1 [Miniussi, A.; Puget, J. -L.; Pajot, F.; Vibert, L.] Univ Paris 11, IAS, F-91405 Orsay, France.
[Holmes, W.] CALTECH, JPL, Pasadena, CA 91125 USA.
[Patanchon, G.; Giraud-Heraud, Y.; Piat, M.] APC, F-75205 Paris 13, France.
[Catalano, A.] LPSC, F-38026 Grenoble, France.
RP Miniussi, A (reprint author), Univ Paris 11, IAS, Bt 121, F-91405 Orsay, France.
EM antoine.miniussi@ias.u-psud.fr
NR 8
TC 1
Z9 1
U1 1
U2 4
PU SPRINGER/PLENUM PUBLISHERS
PI NEW YORK
PA 233 SPRING ST, NEW YORK, NY 10013 USA
SN 0022-2291
EI 1573-7357
J9 J LOW TEMP PHYS
JI J. Low Temp. Phys.
PD SEP
PY 2014
VL 176
IS 5-6
BP 815
EP 821
DI 10.1007/s10909-014-1104-x
PG 7
WC Physics, Applied; Physics, Condensed Matter
SC Physics
GA AM5DE
UT WOS:000339875400029
ER
PT J
AU Staguhn, J
Benford, D
Dwek, E
Hilton, G
Fixsen, D
Irwin, K
Jhabvala, C
Kovacs, A
Leclercq, S
Maher, S
Miller, T
Moseley, SH
Sharp, E
Wollack, E
AF Staguhn, Johannes
Benford, Dominic
Dwek, Eli
Hilton, Gene
Fixsen, Dale
Irwin, Kent
Jhabvala, Christine
Kovacs, Attila
Leclercq, Samuel
Maher, Stephen
Miller, Tim
Moseley, S. Harvey
Sharp, Elmer
Wollack, Edward
TI Design and Expected Performance of GISMO-2, a Two Color Millimeter
Camera for the IRAM 30 m Telescope
SO JOURNAL OF LOW TEMPERATURE PHYSICS
LA English
DT Article
ID INFRARED ASTRONOMY; ARRAYS
AB We present the main design features for the GISMO-2 bolometer camera, which we build for background-limited operation at the IRAM 30 m telescope on Pico Veleta, Spain. GISMO-2 will operate simultaneously in the 1 and 2 mm atmospherical windows. The 1 mm channel uses a TES-based backshort under grid (BUG) bolometer array, the 2 mm channel operates with a BUG array. The camera utilizes almost the entire full field of view provided by the telescope. The optical design of GISMO-2 was strongly influenced by our experience with the GISMO 2 mm bolometer camera, which is successfully operating at the 30 m telescope. GISMO is accessible to the astronomical community through the regular IRAM call for proposals.
C1 [Staguhn, Johannes] Johns Hopkins Univ, Henry A Rowland Dept Phys & Astron, Baltimore, MD 21218 USA.
[Staguhn, Johannes; Benford, Dominic; Dwek, Eli; Fixsen, Dale; Jhabvala, Christine; Maher, Stephen; Miller, Tim; Moseley, S. Harvey; Sharp, Elmer; Wollack, Edward] NASA, Goddard Space Flight Ctr, Observat Cosmol Lab, Greenbelt, MD 20771 USA.
[Hilton, Gene; Irwin, Kent] NIST Quantum Devices Grp, Boulder, CO 80305 USA.
[Kovacs, Attila] Univ Minnesota, Minneapolis, MN 55455 USA.
[Kovacs, Attila] CALTECH, Pasadena, CA 91125 USA.
[Leclercq, Samuel] Inst Radio Astron Millimetr, F-38406 St Martin Dheres, France.
RP Staguhn, J (reprint author), Johns Hopkins Univ, Henry A Rowland Dept Phys & Astron, 3400 N Charles St, Baltimore, MD 21218 USA.
EM johannes.staguhn@nasa.gov
RI Kovacs, Attila/C-1171-2010; Wollack, Edward/D-4467-2012; Benford,
Dominic/D-4760-2012
OI Kovacs, Attila/0000-0001-8991-9088; Wollack, Edward/0000-0002-7567-4451;
Benford, Dominic/0000-0002-9884-4206
FU NSF ATI [1020981, 1106284]
FX This work was supported through NSF ATI grants 1020981 and 1106284.
NR 8
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U1 0
U2 1
PU SPRINGER/PLENUM PUBLISHERS
PI NEW YORK
PA 233 SPRING ST, NEW YORK, NY 10013 USA
SN 0022-2291
EI 1573-7357
J9 J LOW TEMP PHYS
JI J. Low Temp. Phys.
PD SEP
PY 2014
VL 176
IS 5-6
BP 829
EP 834
DI 10.1007/s10909-014-1086-8
PG 6
WC Physics, Applied; Physics, Condensed Matter
SC Physics
GA AM5DE
UT WOS:000339875400031
ER
PT J
AU Hailey-Dunsheath, S
Barry, PS
Bradford, CM
Chattopadhyay, G
Day, P
Doyle, S
Hollister, M
Kovacs, A
LeDuc, HG
Llombart, N
Mauskopf, P
McKenney, C
Monroe, R
Nguyen, HT
O'Brient, R
Padin, S
Reck, T
Shirokoff, E
Swenson, L
Tucker, CE
Zmuidzinas, J
AF Hailey-Dunsheath, S.
Barry, P. S.
Bradford, C. M.
Chattopadhyay, G.
Day, P.
Doyle, S.
Hollister, M.
Kovacs, A.
LeDuc, H. G.
Llombart, N.
Mauskopf, P.
McKenney, C.
Monroe, R.
Nguyen, H. T.
O'Brient, R.
Padin, S.
Reck, T.
Shirokoff, E.
Swenson, L.
Tucker, C. E.
Zmuidzinas, J.
TI Optical Measurements of SuperSpec: A Millimeter-Wave On-Chip
Spectrometer
SO JOURNAL OF LOW TEMPERATURE PHYSICS
LA English
DT Article
DE Kinetic inductance detector; Millimeter-wave; Spectroscopy
AB SuperSpec is a novel on-chip spectrometer we are developing for (sub)millimeter wavelength astronomy. Our approach utilizes a filterbank of moderate resolution ( channels, coupled to lumped element kinetic inductance detectors (KIDs), all integrated onto a single silicon chip. The channels are half-wave resonators formed by lithographically depositing segments of superconducting transmission line, and the KIDs are titanium nitride resonators. Here we present optical measurements of a first generation prototype, operating in the 180-280 GHz frequency range. We have used a coherent source to measure the spectral profiles of 17 channels, which achieve linewidths corresponding to quality factors as high as consistent with the designed values plus additional dissipation characterized by We have also used a Fourier Transform Spectrometer to characterize the spectral purity of all 72 channels on the chip, and measure typical out of band responses dB below the peak response.
C1 [Hailey-Dunsheath, S.; Hollister, M.; Kovacs, A.; McKenney, C.; O'Brient, R.; Padin, S.; Shirokoff, E.; Swenson, L.; Zmuidzinas, J.] CALTECH, Pasadena, CA 91125 USA.
[Barry, P. S.; Doyle, S.; Tucker, C. E.] Cardiff Univ, Sch Phys & Astron, Cardiff CF24 3AA, S Glam, Wales.
[Bradford, C. M.; Chattopadhyay, G.; Day, P.; LeDuc, H. G.; Monroe, R.; Nguyen, H. T.; Reck, T.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Kovacs, A.] Univ Minnesota, Inst Astrophys, Minneapolis, MN 55455 USA.
[Llombart, N.] Univ Complutense Madrid, Dept Opt, Madrid 28037, Spain.
[Mauskopf, P.] Arizona State Univ, Tempe, AZ 85287 USA.
RP Hailey-Dunsheath, S (reprint author), CALTECH, Mail Code 301-17,1200 E Calif Blvd, Pasadena, CA 91125 USA.
EM haileyds@caltech.edu
RI Kovacs, Attila/C-1171-2010
OI Kovacs, Attila/0000-0001-8991-9088
FU NASA Astrophysics Research and Analysis (APRA) [399131.02.06.03.43]; W.
M. Keck Institute for Space Studies; NASA Postdoctoral Program; Science
and Technology Facilities Council [ST/G002711/1, ST/J001449/1]
FX This project is supported by NASA Astrophysics Research and Analysis
(APRA) Grant No. 399131.02.06.03.43. ES, CMM, and LJS acknowledge
support from the W. M. Keck Institute for Space Studies. MIH, LJS, and
TR acknowledge support from the NASA Postdoctoral Program. PSB
acknowledges the continuing support from the Science and Technology
Facilities Council Ph.D studentship programme and grant programmes
ST/G002711/1 and ST/J001449/1. Device fabrication was performed the JPL
Microdevices Laboratory.
NR 7
TC 3
Z9 3
U1 0
U2 3
PU SPRINGER/PLENUM PUBLISHERS
PI NEW YORK
PA 233 SPRING ST, NEW YORK, NY 10013 USA
SN 0022-2291
EI 1573-7357
J9 J LOW TEMP PHYS
JI J. Low Temp. Phys.
PD SEP
PY 2014
VL 176
IS 5-6
BP 841
EP 847
DI 10.1007/s10909-013-1068-2
PG 7
WC Physics, Applied; Physics, Condensed Matter
SC Physics
GA AM5DE
UT WOS:000339875400033
ER
PT J
AU Ferri, E
Bagliani, D
Biassotti, M
Ceruti, G
Corsini, D
Faverzani, M
Gatti, F
Giachero, A
Gotti, C
Kilbourne, C
Kling, A
Kraft-Bermuth, S
Maino, M
Manfrinetti, P
Nucciotti, A
Pessina, G
Pizzigoni, G
Gomes, MR
Schaeffer, D
Sisti, M
AF Ferri, E.
Bagliani, D.
Biassotti, M.
Ceruti, G.
Corsini, D.
Faverzani, M.
Gatti, F.
Giachero, A.
Gotti, C.
Kilbourne, C.
Kling, A.
Kraft-Bermuth, S.
Maino, M.
Manfrinetti, P.
Nucciotti, A.
Pessina, G.
Pizzigoni, G.
Ribeiro Gomes, M.
Schaeffer, D.
Sisti, M.
TI Preliminary Results of the MARE Experiment
SO JOURNAL OF LOW TEMPERATURE PHYSICS
LA English
DT Article
DE Thermal detectors; Neutrino mass; Single beta decay; Electron capture
ID NEUTRINO MASS EXPERIMENT; MICROCALORIMETERS; SEARCH; MILAN
AB The microcalorimeter array for a rhenium experiment (MARE) project aims at the direct and calorimetric measurement of the electron neutrino mass with sub-eV sensitivity. The design is based on large arrays of thermal detectors to study the beta decay of Re and the electron capture of Ho. One of the activities of the project, MARE 1 in Milan, has started in Milan using one array of 6 6 silicon implanted thermistors equipped with AgReO absorbers. The purposes of MARE 1 in Milan are to achieve a sensitivity on the neutrino mass of a few eV and to investigate the systematics of Re neutrino mass measurements, focusing on those caused by the beta environmental fine structure and the beta spectrum theoretical shape. In parallel, the MARE collaboration is performing an R&D work for producing absorbers embedded with radioactive metal Ho. We report here the status of MARE using Re as beta source and the preliminary results obtained with Ho-163.
C1 [Ferri, E.; Ceruti, G.; Faverzani, M.; Giachero, A.; Gotti, C.; Maino, M.; Nucciotti, A.; Pessina, G.; Sisti, M.] Univ Milano Bicocca, Milan, Italy.
[Ferri, E.; Ceruti, G.; Faverzani, M.; Giachero, A.; Gotti, C.; Maino, M.; Nucciotti, A.; Pessina, G.; Sisti, M.] Ist Nazl Fis Nucl, Sez Milan Bicocca, I-20133 Milan, Italy.
[Bagliani, D.; Biassotti, M.; Corsini, D.; Gatti, F.; Manfrinetti, P.; Pizzigoni, G.] Univ Genoa, Genoa, Italy.
[Bagliani, D.; Biassotti, M.; Corsini, D.; Gatti, F.; Manfrinetti, P.; Pizzigoni, G.] Ist Nazl Fis Nucl, Sez Genoa, I-16146 Genoa, Italy.
[Kilbourne, C.] NASA, Goddard Space Flight Ctr, Greenbelt, MA USA.
[Kling, A.; Ribeiro Gomes, M.] Univ Lisbon, Ctr Nucl Phys, P-1699 Lisbon, Portugal.
[Kling, A.] IST ID, Lisbon, Portugal.
[Kraft-Bermuth, S.] Johannes Gutenberg Univ Mainz, Inst Phys, Mainz, Germany.
[Schaeffer, D.] ABB AB, Corp Res, Vasteras, Sweden.
RP Ferri, E (reprint author), Univ Milano Bicocca, Milan, Italy.
EM elena.ferri@mib.infn.it
RI Giachero, Andrea/I-1081-2013; Nucciotti, Angelo/I-8888-2012; Ferri,
Elena/L-8531-2014; Kling, Andreas/C-1115-2012; Kraft-Bermuth,
Saskia/G-4007-2012; Sisti, Monica/B-7550-2013; Faverzani,
Marco/K-3865-2016;
OI Giachero, Andrea/0000-0003-0493-695X; Nucciotti,
Angelo/0000-0002-8458-1556; Ferri, Elena/0000-0003-1425-3669; Kling,
Andreas/0000-0002-5597-502X; Kraft-Bermuth, Saskia/0000-0002-0864-7912;
Sisti, Monica/0000-0003-2517-1909; Faverzani, Marco/0000-0001-8119-2953;
Pessina, Gianluigi Ezio/0000-0003-3700-9757; Gotti,
Claudio/0000-0003-2501-9608
FU Fondazione Cariplo through the project Development of Microresonator
Detectors for Neutrino Physics [2010-2351]; Marie Curie Actions
[FP7-PEOPLE-2007-2-2-ERG]; FCT-Portugal programs [PTDC-FIS-116719-2010]
FX These activities are supported by Fondazione Cariplo through the project
Development of Microresonator Detectors for Neutrino Physics (Grant
2010-2351). The MARE-Ho work was partially supported by the Marie Curie
Actions (FP7-PEOPLE-2007-2-2-ERG) and FCT-Portugal programs (Project
PTDC-FIS-116719-2010).
NR 12
TC 7
Z9 7
U1 0
U2 12
PU SPRINGER/PLENUM PUBLISHERS
PI NEW YORK
PA 233 SPRING ST, NEW YORK, NY 10013 USA
SN 0022-2291
EI 1573-7357
J9 J LOW TEMP PHYS
JI J. Low Temp. Phys.
PD SEP
PY 2014
VL 176
IS 5-6
BP 885
EP 890
DI 10.1007/s10909-013-1026-z
PG 6
WC Physics, Applied; Physics, Condensed Matter
SC Physics
GA AM5DE
UT WOS:000339875400038
ER
PT J
AU Cornell, B
Moore, DC
Golwala, SR
Bumble, B
Day, PK
LeDuc, HG
Zmuidzinas, J
AF Cornell, B.
Moore, D. C.
Golwala, S. R.
Bumble, B.
Day, P. K.
LeDuc, H. G.
Zmuidzinas, J.
TI Particle Detection Using MKID-Based Athermal-Phonon Mediated Detectors
SO JOURNAL OF LOW TEMPERATURE PHYSICS
LA English
DT Article
DE Kinetic inductance detectors; Phonon; Rare event search; MKID
AB We are developing athermal-phonon mediated particle detectors that utilize microwave kinetic inductance detectors (MKIDs) as phonon sensors. MKIDs afford natural frequency domain multiplexing, which allows for massive substrates to be patterned with hundreds of sensors while keeping readout complexity to a minimum. Previously, our 2 cm 2 cm 1 mm proof-of-principle device utilized 20 MKIDs and, from the magnitude and timing of their response, we were able to reconstruct the position of a particle interaction to 1 mm. From this, we corrected for variations in detector response across the device and measured an energy resolution of keV at 30 keV. We have designed and fabricated a new 3-inch prototype device that utilizes 256 MKID sensors, and we present results from its initial testing. Applications include rare event searches, such as the direct detection of dark matter and neutrinoless double beta decay, as well as hard X-ray/soft -ray astrophysics.
C1 [Cornell, B.; Moore, D. C.; Golwala, S. R.; Zmuidzinas, J.] CALTECH, Pasadena, CA 91125 USA.
[Bumble, B.; Day, P. K.; LeDuc, H. G.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Cornell, B (reprint author), CALTECH, 1200 E Calif Blvd, Pasadena, CA 91125 USA.
EM cornell@caltech.edu
FU Gordon and Betty Moore Foundation; NASA
FX Our research was carried out primarily at the Jet Propulsion Laboratory
(JPL) and the California Institute for Technology, under contract from
NASA. JPL's Microdevices Laboratory fabricated the devices used in this
work. We would like to acknowledge the generous support of the Gordon
and Betty Moore Foundation. Our work benefited greatly from the
expertise of, as well as software developed by, the CDMS/SuperCDMS
collaboration for the development of phonon-mediated particle detectors.
We would also like to thank NASA's Space Technology Research Fellowship
program for its ongoing support.
NR 10
TC 1
Z9 1
U1 1
U2 7
PU SPRINGER/PLENUM PUBLISHERS
PI NEW YORK
PA 233 SPRING ST, NEW YORK, NY 10013 USA
SN 0022-2291
EI 1573-7357
J9 J LOW TEMP PHYS
JI J. Low Temp. Phys.
PD SEP
PY 2014
VL 176
IS 5-6
BP 891
EP 897
DI 10.1007/s10909-013-1039-7
PG 7
WC Physics, Applied; Physics, Condensed Matter
SC Physics
GA AM5DE
UT WOS:000339875400039
ER
PT J
AU Kraft-Bermuth, S
Andrianov, V
Bleile, A
Echler, A
Egelhof, P
Grabitz, P
Kilbourne, C
Kiselev, O
McCammon, D
Scholz, P
AF Kraft-Bermuth, S.
Andrianov, V.
Bleile, A.
Echler, A.
Egelhof, P.
Grabitz, P.
Kilbourne, C.
Kiselev, O.
McCammon, D.
Scholz, P.
TI Precise Determination of the Lyman-1 Transition Energy in Hydrogen-like
Gold Ions with Microcalorimeters
SO JOURNAL OF LOW TEMPERATURE PHYSICS
LA English
DT Article
DE Microcalorimeters for X-rays; Precision test of QED; Highly-charged ions
ID X-RAY SPECTROSCOPY; LOW-TEMPERATURE DETECTORS; HEAVY-IONS
AB The precise determination of the transition energy of the Lyman-1 line in hydrogen-like heavy ions provides a sensitive test of quantum electrodynamics in very strong Coulomb fields. We report the determination of the Lyman-1 transition energy of gold ions (Au) with microcalorimeters at the experimental storage ring at GSI. X-rays produced by the interaction of 125 MeV/u Au ions with an internal argon gas-jet target were detected. The detector array consisted of 14 pixels with silicon thermistors and Sn absorbers, for which an energy resolution of 50 eV for an X-ray energy of 59.5 keV was obtained in the laboratory. The Lyman-1 transition energy was determined for each pixel in the laboratory frame, then transformed into the emitter frame and averaged. A Dy-159 source was used for energy calibration. The absolute positions of the detector pixels, which are needed for an accurate correction of the Doppler shift, were determined by topographic measurements and by scanning a collimated Am-241 source across the cryostat window. The energy of the Lyman-1 line in the emitter frame is eV, in good agreement with theoretical predictions. The systematic error is dominated by the uncertainty in the position of the cryostat relative to the interaction region of beam and target.
C1 [Kraft-Bermuth, S.; Echler, A.; Scholz, P.] Univ Giessen, Inst Atom Phys, D-35390 Giessen, Germany.
[Andrianov, V.; Bleile, A.; Echler, A.; Egelhof, P.; Grabitz, P.; Kiselev, O.] GSI Helmholtzzentrum, Darmstadt, Germany.
[Andrianov, V.] Moscow MV Lomonosov State Univ, Inst Nucl Phys, Moscow, Russia.
[Egelhof, P.; Grabitz, P.] Johannes Gutenberg Univ Mainz, D-55122 Mainz, Germany.
[Kilbourne, C.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[McCammon, D.] Univ Wisconsin, Dept Phys, Madison, WI 53706 USA.
RP Kraft-Bermuth, S (reprint author), Univ Giessen, Inst Atom Phys, D-35390 Giessen, Germany.
EM saskia.kraft-bermuth@iamp.physik.uni-giessen.de
RI Kraft-Bermuth, Saskia/G-4007-2012
OI Kraft-Bermuth, Saskia/0000-0002-0864-7912
FU Deutsche Forschungsgemeinschaft (DFG)
FX We thank K. Eberhard and J. Runke from the Institute of Nuclear
Chemistry of the Johannes Gutenberg Universitat Mainz for producing the
Dy-159 source. We also thank our co-experimentators from the FOCAL group
for good cooperation during the measurements. The ESR group of GSI
provided us with stable experimental conditions. This work was supported
by the Emmy Noether Young Researchers Program of the Deutsche
Forschungsgemeinschaft (DFG).
NR 12
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U1 0
U2 8
PU SPRINGER/PLENUM PUBLISHERS
PI NEW YORK
PA 233 SPRING ST, NEW YORK, NY 10013 USA
SN 0022-2291
EI 1573-7357
J9 J LOW TEMP PHYS
JI J. Low Temp. Phys.
PD SEP
PY 2014
VL 176
IS 5-6
BP 1002
EP 1008
DI 10.1007/s10909-013-1002-7
PG 7
WC Physics, Applied; Physics, Condensed Matter
SC Physics
GA AM5DE
UT WOS:000339875400055
ER
PT J
AU Heine, SNT
Figueroa-Feliciano, E
Rutherford, JM
Wikus, P
Oakley, P
Porter, FS
McCammon, D
AF Heine, S. N. T.
Figueroa-Feliciano, E.
Rutherford, J. M.
Wikus, P.
Oakley, P.
Porter, F. S.
McCammon, D.
TI Vibration Isolation Design for the Micro-X Rocket Payload
SO JOURNAL OF LOW TEMPERATURE PHYSICS
LA English
DT Article
DE Vibration isolation; Transition-edge sensors; Sounding rockets; X-ray
spectrometers
ID MICROCALORIMETERS
AB Micro-X is a NASA-funded, sounding rocket-borne X-ray imaging spectrometer that will allow high precision measurements of velocity structure, ionization state and elemental composition of extended astrophysical systems. One of the biggest challenges in payload design is to maintain the temperature of the detectors during launch. There are several vibration damping stages to prevent energy transmission from the rocket skin to the detector stage, which causes heating during launch. Each stage should be more rigid than the outer stages to achieve vibrational isolation. We describe a major design effort to tune the resonance frequencies of these vibration isolation stages to reduce heating problems prior to the projected launch in the summer of 2014.
C1 [Heine, S. N. T.; Figueroa-Feliciano, E.; Rutherford, J. M.; Wikus, P.; Oakley, P.; Porter, F. S.; McCammon, D.] MIT, MIT Kavli Inst, Cambridge, MA 02139 USA.
[Porter, F. S.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[McCammon, D.] Univ Wisconsin, Madison, WI USA.
RP Heine, SNT (reprint author), MIT, MIT Kavli Inst, 77 Massachusetts Ave, Cambridge, MA 02139 USA.
EM saraht@mit.edu
RI Porter, Frederick/D-3501-2012
OI Porter, Frederick/0000-0002-6374-1119
NR 5
TC 3
Z9 3
U1 0
U2 3
PU SPRINGER/PLENUM PUBLISHERS
PI NEW YORK
PA 233 SPRING ST, NEW YORK, NY 10013 USA
SN 0022-2291
EI 1573-7357
J9 J LOW TEMP PHYS
JI J. Low Temp. Phys.
PD SEP
PY 2014
VL 176
IS 5-6
BP 1082
EP 1088
DI 10.1007/s10909-013-1032-1
PG 7
WC Physics, Applied; Physics, Condensed Matter
SC Physics
GA AM5DE
UT WOS:000339875400066
ER
PT J
AU Doude, HR
Schneider, JA
Nunes, AC
AF Doude, Haley R.
Schneider, Judy A.
Nunes, Arthur C., Jr.
TI Influence of the Tool Shoulder Contact Conditions on the Material Flow
During Friction Stir Welding
SO METALLURGICAL AND MATERIALS TRANSACTIONS A-PHYSICAL METALLURGY AND
MATERIALS SCIENCE
LA English
DT Article
ID TEMPERATURE DISTRIBUTION; MECHANICAL-PROPERTIES; ALUMINUM-ALLOYS;
HEAT-TRANSFER; PROCESS MODEL; ONION RINGS; METAL FLOW; MICROSTRUCTURE;
VISUALIZATION; GEOMETRY
AB Friction stir welding (FSWing) is a solid-state joining process of special interest in joining alloys that are traditionally difficult to fusion weld. In order to optimize the process, various numeric modeling approaches have been pursued. Of importance to furthering modeling efforts is a better understanding of the contact conditions between the workpiece and the weld tool. Both theoretical and experimental studies indicate the contact conditions between the workpiece and weld tool are unknown, possibly varying during the FSW process. To provide insight into the contact conditions, this study characterizes the material flow in the FSW nugget by embedding a lead (Pb) wire that melted at the FSWing temperature of aluminum alloy 2195. The Pb trace provided evidence of changes in material flow characteristics which were attributed to changes in the contact conditions between the weld tool and workpiece, as driven by temperature, as the tool travels the length of a weld seam.
C1 [Doude, Haley R.] Mississippi State Univ, Ctr Adv Vehicular Syst, Mississippi State, MS 39762 USA.
[Schneider, Judy A.] Mississippi State Univ, Dept Mech Engn, Mississippi State, MS 39762 USA.
[Nunes, Arthur C., Jr.] NASA, MSFC, Huntsville, AL USA.
RP Doude, HR (reprint author), Mississippi State Univ, Ctr Adv Vehicular Syst, Mississippi State, MS 39762 USA.
EM har15@msstate.edu
FU NASA Faculty Fellowship Program; NASA GSRP Fellowship
FX The authors [HRD, JAS] acknowledge the funding support provided by the
NASA Faculty Fellowship Program and a NASA GSRP Fellowship [HRD].
NR 51
TC 6
Z9 6
U1 9
U2 43
PU SPRINGER
PI NEW YORK
PA 233 SPRING ST, NEW YORK, NY 10013 USA
SN 1073-5623
EI 1543-1940
J9 METALL MATER TRANS A
JI Metall. Mater. Trans. A-Phys. Metall. Mater. Sci.
PD SEP
PY 2014
VL 45A
IS 10
BP 4411
EP 4422
DI 10.1007/s11661-014-2384-0
PG 12
WC Materials Science, Multidisciplinary; Metallurgy & Metallurgical
Engineering
SC Materials Science; Metallurgy & Metallurgical Engineering
GA AM5HP
UT WOS:000339888100026
ER
PT J
AU Jones, SF
Blain, AW
Stern, D
Assef, RJ
Bridge, CR
Eisenhardt, P
Petty, S
Wu, JW
Tsai, CW
Cutri, R
Wright, EL
Yan, L
AF Jones, Suzy F.
Blain, Andrew W.
Stern, Daniel
Assef, Roberto J.
Bridge, Carrie R.
Eisenhardt, Peter
Petty, Sara
Wu, Jingwen
Tsai, Chao-Wei
Cutri, Roc
Wright, Edward L.
Yan, Lin
TI Submillimetre observations of WISE-selected high-redshift, luminous,
dusty galaxies
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE galaxies: active; galaxies: formation; galaxies: high-redshift;
infrared: galaxies; submillimetre: galaxies
ID ULTRALUMINOUS INFRARED GALAXIES; ACTIVE GALACTIC NUCLEI; SPECTRAL
ENERGY-DISTRIBUTIONS; DEGREE EXTRAGALACTIC SURVEY; SUPERMASSIVE
BLACK-HOLES; OBSCURED STAR-FORMATION; MU-M OBSERVATIONS;
DEEP-FIELD-SOUTH; NUMBER COUNTS; XMM-NEWTON
AB We present SCUBA-2 (Submillimetre Common-User Bolometer Array) 850 mu m submillimetre (submm) observations of the fields of 10 dusty, luminous galaxies at z similar to 1.7-4.6, detected at 12 and/or 22 mu m by the Wide-field Infrared Survey Explorer (WISE) all-sky survey, but faint or undetected at 3.4 and 4.6 mu m; dubbed hot, dust-obscured galaxies (Hot DOGs). The six detected targets all have total infrared luminosities greater than 10(13) L-aS (TM), with one greater than 10(14) L-aS (TM). Their spectral energy distributions (SEDs) are very blue from mid-infrared to submm wavelengths and not well fitted by standard active galactic nuclei (AGN) SED templates, without adding extra dust extinction to fit the WISE 3.4 and 4.6 mu m data. The SCUBA-2 850 mu m observations confirm that the Hot DOGs have less cold and/or more warm dust emission than standard AGN templates, and limit an underlying extended spiral or ULIRG-type galaxy to contribute less than about 2 or 55 per cent of the typical total Hot DOG IR luminosity, respectively. The two most distant and luminous targets have similar observed submm to mid-infrared ratios to the rest, and thus appear to have even hotter SEDs. The number of serendipitous submm galaxies detected in the 1.5-arcmin-radius SCUBA-2 850 mu m maps indicates there is a significant overdensity of serendipitous sources around Hot DOGs. These submm observations confirm that the WISE-selected ultraluminous galaxies have very blue mid-infrared to submm SEDs, suggesting that they contain very powerful AGN, and are apparently located in unusual arcmin-scale overdensities of very luminous dusty galaxies.
C1 [Jones, Suzy F.; Blain, Andrew W.] Univ Leicester, Xray & Observat Astron Grp XROA, Dept Phys & Astron, Leicester LE1 7RH, Leics, England.
[Stern, Daniel; Eisenhardt, Peter; Tsai, Chao-Wei] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Assef, Roberto J.] Univ Diego Portales, Fac Ingn, Nucleo Astron, Santiago, Chile.
[Bridge, Carrie R.] CALTECH, Pasadena, CA 91125 USA.
[Petty, Sara] Virginia Polytech Inst & State Univ, Dept Phys, Blacksburg, VA 24061 USA.
[Wu, Jingwen; Wright, Edward L.] Univ Calif Los Angeles, Div Phys & Astron, Los Angeles, CA 90095 USA.
[Cutri, Roc; Yan, Lin] CALTECH, Infrared Proc & Anal Ctr, Pasadena, CA 91125 USA.
RP Jones, SF (reprint author), Univ Leicester, Xray & Observat Astron Grp XROA, Dept Phys & Astron, Univ Rd, Leicester LE1 7RH, Leics, England.
EM sfj8@le.ac.uk
FU University of Leicester Physics & Astronomy Department; Gemini-CONICYT
[32120009]; National Aeronautics and Space Administration; Canada
Foundation for Innovation; [M12AU010]
FX SFJ gratefully acknowledges support from the University of Leicester
Physics & Astronomy Department. RJA was supported by Gemini-CONICYT
grant number 32120009. This publication makes use of data products from
the WISE, 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.; The James Clerk Maxwell Telescope is operated by the
Joint Astronomy Centre on behalf of the Science and Technology
Facilities Council of the United Kingdom, the Netherlands Organization
for Scientific Research, and the National Research Council of Canada.
Additional funds for the construction of SCUBA-2 were provided by the
Canada Foundation for Innovation. The project ID under which the data
were obtained was M12AU010.
NR 85
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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 SEP 1
PY 2014
VL 443
IS 1
BP 146
EP 157
DI 10.1093/mnras/stu1157
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AM5UR
UT WOS:000339927000014
ER
PT J
AU Gorbikov, E
Gal-Yam, A
Ofek, EO
Vreeswijk, PM
Nugent, PE
Chotard, N
Kulkarni, SR
Cao, Y
De Cia, A
Yaron, O
Tal, D
Arcavi, I
Kasliwal, MM
Cenko, SB
Sullivan, M
Chen, JC
AF Gorbikov, Evgeny
Gal-Yam, Avishay
Ofek, Eran O.
Vreeswijk, Paul M.
Nugent, Peter E.
Chotard, Nicolas
Kulkarni, Shrinivas R.
Cao, Yi
De Cia, Annalisa
Yaron, Ofer
Tal, David
Arcavi, Iair
Kasliwal, Mansi M.
Cenko, S. Bradley
Sullivan, Mark
Chen, Juncheng
TI iPTF13beo: the double-peaked light curve of a Type Ibn supernova
discovered shortly after explosion
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE supernovae: general; supernovae: individual: iPTF13beo; stars: winds,
outflows; stars: Wolf-Rayet
ID RICH CIRCUMSTELLAR MEDIUM; SN 2009IP; SHOCK BREAKOUT; DUST FORMATION;
CORE-COLLAPSE; MASSIVE STAR; 2006JC; EMISSION; OUTBURST; SPECTROSCOPY
AB We present optical photometric and spectroscopic observations of the Type Ibn (SN 2006jc-like) supernova (SN) iPTF13beo. Detected by the intermediate Palomar Transient Factory similar to 3 h after the estimated first light, iPTF13beo is the youngest and the most distant (similar to 430 Mpc) Type Ibn event ever observed. The iPTF13beo light curve is consistent with light curves of other Type Ibn SNe and with light curves of fast Type Ic events, but with a slightly faster rise-time of two days. In addition, the iPTF13beo R-band light curve exhibits a double-peak structure separated by similar to 9 d, not observed before in any Type Ibn SN. A low-resolution spectrum taken during the iPTF13beo rising stage is featureless, while a late-time spectrum obtained during the declining stage exhibits narrow and intermediate-width He i and Si ii features with full width at half-maximum a parts per thousand 2000-5000 km s(-1) and is remarkably similar to the prototypical SN Ibn 2006jc spectrum. We suggest that our observations support a model of a massive star exploding in a dense He-rich circumstellar medium (CSM). A shock breakout in a CSM model requires an eruption releasing a total mass of similar to 0.1 MaS (TM) over a time-scale of couple of weeks prior to the SN explosion.
C1 [Gorbikov, Evgeny; Gal-Yam, Avishay; Ofek, Eran O.; Vreeswijk, Paul M.; De Cia, Annalisa; Yaron, Ofer; Tal, David; Arcavi, Iair] Weizmann Inst Sci, Fac Phys, Benoziyo Ctr Astrophys, IL-76100 Rehovot, Israel.
[Nugent, Peter E.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA.
[Nugent, Peter E.] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Computat Res Div, Computat Cosmol Ctr, Berkeley, CA 94720 USA.
[Chotard, Nicolas] Univ Lyon, F-69622 Lyon, France.
[Chotard, Nicolas] Univ Lyon 1, F-69622 Villeurbanne, France.
[Chotard, Nicolas] CNRS, IN2P3, Inst Phys Nucl Lyon, F-75700 Paris, France.
[Kulkarni, Shrinivas R.; Cao, Yi] CALTECH, Dept Astron, Pasadena, CA 91125 USA.
[Kasliwal, Mansi M.] Carnegie Inst Sci, Pasadena, CA 91101 USA.
[Cenko, S. Bradley] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA.
[Cenko, S. Bradley] Univ Maryland, Joint Space Sci Inst, College Pk, MD 20742 USA.
[Sullivan, Mark] Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England.
[Chen, Juncheng] Tsinghua Univ, Tsinghua Ctr Astrophys, Beijing 100084, Peoples R China.
RP Gorbikov, E (reprint author), Weizmann Inst Sci, Fac Phys, Benoziyo Ctr Astrophys, IL-76100 Rehovot, Israel.
EM mrmagnate@mail.ru
OI Sullivan, Mark/0000-0001-9053-4820
FU W. M. Keck Foundation; Israeli Ministry of Science; I-CORE Programme of
the Planning and Budgeting Committee; Israel Science Foundation
[1829/12]; EU/FP7 via ERC grant [307260]; ISF grant; BSF grant; Minerva
grant; GIF grant; ISF; Israeli Planning and Budgeting Committee; Kimmel
award; Lyon Institute of Origins [ANR-10-LABX-66]
FX This paper is based on observations obtained with the Samuel Oschin
Telescope as part of the Palomar Transient Factory project, a scientific
collaboration between the California Institute of Technology, Columbia
University, Las Cumbres Observatory, the Lawrence Berkeley National
Laboratory, the National Energy Research Scientific Computing Center,
the University of Oxford, and the Weizmann Institute of Science. Some of
the data presented herein 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
Observatory was made possible by the generous financial support of the
W. M. Keck Foundation. We are grateful for excellent staff assistance at
Palomar, Lick, and Keck Observatories. EOO is incumbent of the Arye
Dissentshik career development chair and is grateful to support by a
grant from the Israeli Ministry of Science and the I-CORE Programme of
the Planning and Budgeting Committee and The Israel Science Foundation
(grant no. 1829/12).; AG-Y acknowledges support by the EU/FP7 via ERC
grant no. 307260, ISF, BSF, Minerva and GIF grants, the 'Quantum
Universe' I-Core programme funded by the ISF and the Israeli Planning
and Budgeting Committee, and the Kimmel award.; NC acknowledges support
from the Lyon Institute of Origins under grant ANR-10-LABX-66.
NR 45
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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 SEP 1
PY 2014
VL 443
IS 1
BP 671
EP 677
DI 10.1093/mnras/stu1184
PG 7
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AM5UR
UT WOS:000339927000052
ER
PT J
AU Snyder, TJ
Andrews, M
Weislogel, M
Moeck, P
Stone-Sundberg, J
Birkes, D
Hoffert, MP
Lindeman, A
Morrill, J
Fercak, O
Friedman, S
Gunderson, J
Ha, A
McCollister, J
Chen, YK
Geile, J
Wollman, A
Attari, B
Botnen, N
Vuppuluri, V
Shim, J
Kaminsky, W
Adams, D
Graft, J
AF Snyder, Trevor J.
Andrews, Mike
Weislogel, Mark
Moeck, Peter
Stone-Sundberg, Jennifer
Birkes, Derek
Hoffert, Madeline Paige
Lindeman, Adam
Morrill, Jeff
Fercak, Ondrej
Friedman, Sasha
Gunderson, Jeff
Ha, Anh
McCollister, Jack
Chen, Yongkang
Geile, John
Wollman, Andrew
Attari, Babak
Botnen, Nathan
Vuppuluri, Vasant
Shim, Jennifer
Kaminsky, Werner
Adams, Dustin
Graft, John
TI 3D Systems' Technology Overview and New Applications in Manufacturing,
Engineering, Science, and Education
SO 3D PRINTING AND ADDITIVE MANUFACTURING
LA English
DT Article
AB Since the inception of 3D printing, an evolutionary process has taken place in which specific user and customer needs have crossed paths with the capabilities of a growing number of machines to create value-added businesses. Even today, over 30 years later, the growth of 3D printing and its utilization for the good of society is often limited by the various users 'understanding of the technology for their specific needs. This article presents an overview of current 3D printing technologies and shows numerous examples from a multitude of fields from manufacturing to education.
C1 [Snyder, Trevor J.; Andrews, Mike] 3D Syst, 26600 SW Pkwy, Wilsonville, OR 97070 USA.
[Weislogel, Mark; Moeck, Peter; Stone-Sundberg, Jennifer; Birkes, Derek; Hoffert, Madeline Paige; Lindeman, Adam; Morrill, Jeff; Fercak, Ondrej; Friedman, Sasha; Gunderson, Jeff; Ha, Anh; McCollister, Jack; Chen, Yongkang; Geile, John; Wollman, Andrew; Attari, Babak; Botnen, Nathan; Vuppuluri, Vasant] Portland State Univ, Portland, OR 97207 USA.
[Shim, Jennifer] Princeton Univ, Princeton, NJ 08544 USA.
[Kaminsky, Werner] Univ Washington, Seattle, WA 98195 USA.
[Adams, Dustin] Xerox Corp, Wilsonville, OR USA.
[Graft, John] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA.
RP Snyder, TJ (reprint author), 3D Syst, 26600 SW Pkwy, Wilsonville, OR 97070 USA.
NR 13
TC 10
Z9 10
U1 5
U2 11
PU MARY ANN LIEBERT, INC
PI NEW ROCHELLE
PA 140 HUGUENOT STREET, 3RD FL, NEW ROCHELLE, NY 10801 USA
SN 2329-7662
EI 2329-7670
J9 3D PRINT ADDIT MANUF
JI 3D Print. Addit. Manuf.
PD SEP
PY 2014
VL 1
IS 3
BP 169
EP 176
DI 10.1089/3dp.2014.1502
PG 8
WC Engineering, Manufacturing; Materials Science, Multidisciplinary
SC Engineering; Materials Science
GA V43BV
UT WOS:000209657800010
ER
PT J
AU Hossain, F
Maswood, M
Siddique-E-Akbor, AH
Yigzaw, W
Mazumder, LC
Ahmed, T
Hossain, M
Shah-Newaz, SM
Limaye, A
Lee, H
Pradhan, S
Shrestha, B
Bajracahrya, B
Biancamaria, S
Shum, CK
Turk, FJ
AF Hossain, Faisal
Maswood, Mehedi
Siddique-E-Akbor, A. H.
Yigzaw, Wondmagegn
Mazumder, Liton Chandra
Ahmed, Tanvir
Hossain, Monowar
Shah-Newaz, S. M.
Limaye, Ashutosh
Lee, Hyongki
Pradhan, Sudip
Shrestha, Basanta
Bajracahrya, Birendra
Biancamaria, Sylvain
Shum, C. K.
Turk, F. J.
TI A Promising Radar Altimetry Satellite System for Operational Flood
Forecasting in Flood-Prone Bangladesh
SO IEEE GEOSCIENCE AND REMOTE SENSING MAGAZINE
LA English
DT Article
AB Building on a recent suite of work that has demonstrated theoretical feasibility and operational readiness of a satellite altimeter based flood forecasting system, we recently put a progressively designed altimeter based transboundary flood forecasting system to the ultimate test of real-time operational delivery in Bangladesh. The JASON-2 satellite altimeter, which was in orbit at the time of writing this manuscript, was used as the flagship altimeter mission. This paper summarizes the entire process of designing the system, customizing the workflow, and putting the system in place for complete ownership by the Bangladesh stakeholder agency for a 100 day operational skill test spanning the period of June 1 2013 through Sept. 9, 2013. Correlation for most of the flood warning stations ranged between 0.95 to 0.80 during the 1 day to 8 days lead time range. The RMSE of forecast typically ranged between 0.75m to 1.5m at locations where the danger level relative to the river bed was more than an order higher (i.e., > 20m). The RMSE of forecast at the 8 days lead time did not exceed 2m for upstream and mid-stream rivers inside Bangladesh. The RMSE of forecast at the 8 days lead time exceeded 2m at a few estuarine river locations affected by tidal effects, where danger level relative to river bed was smaller (i.e., < 20m). Such a satellite altimeter system, such as one based on the JASON-2 altimeter, is now poised to serve the entire inhabitants of the Ganges-Brahmaputra-Meghna river basins as well as 30 or more flood-prone downstream nations currently deprived of real-time flow data from upstream nations.
C1 [Hossain, Faisal; Maswood, Mehedi] Univ Washington, Dept Civil & Environm Engn, Seattle, WA 98195 USA.
[Siddique-E-Akbor, A. H.; Yigzaw, Wondmagegn] Tennessee Technol Univ, Cookeville, TN 38505 USA.
[Mazumder, Liton Chandra; Ahmed, Tanvir; Hossain, Monowar; Shah-Newaz, S. M.] Inst Water Modeling, Dhaka, Bangladesh.
[Limaye, Ashutosh] NASA Marshall Space Flight Ctr, Huntsville, AL USA.
[Lee, Hyongki] Univ Houston, Dept Civil & Environm Engn, Houston, TX 77204 USA.
[Pradhan, Sudip; Shrestha, Basanta; Bajracahrya, Birendra] Int Ctr Integrated Mt Dev ICIMOD, Kathmandu, Nepal.
[Biancamaria, Sylvain] LEGOS, Toulouse, France.
[Shum, C. K.] Ohio State Univ, Sch Earth Sci, Columbus, OH 43210 USA.
[Turk, F. J.] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
RP Hossain, F (reprint author), Univ Washington, Dept Civil & Environm Engn, Seattle, WA 98195 USA.
FU NASA Physical Oceanography program [NN13AD97G]; NASA SERVIR program
[NNX12AM85AG]; Institute of Water Modeling (IWM) in Bangladesh
FX The first author acknowledges the gracious support provided by the US
Department of State (Fulbright Program) for capacity building of
Bangladesh flood forecasting infrastructure. Additional support from
NASA Physical Oceanography program (NN13AD97G) and NASA SERVIR program
(NNX12AM85AG) is also acknowledged. The authors are also grateful to the
generous support received from the Institute of Water Modeling (IWM) in
Bangladesh for access to quality controlled discharge and river level
data as part of a 5-year MOU between TTU and IWM.
NR 16
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PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 2168-6831
J9 IEEE GEOSC REM SEN M
JI IEEE Geosci. Remote Sens. Mag.
PD SEP
PY 2014
VL 2
IS 3
BP 27
EP 36
DI 10.1109/MGRS.2014.2345414
PG 10
WC Geochemistry & Geophysics; Remote Sensing; Imaging Science &
Photographic Technology
SC Geochemistry & Geophysics; Remote Sensing; Imaging Science &
Photographic Technology
GA V45PW
UT WOS:000209829500004
ER
PT J
AU Ely, TA
AF Ely, Todd A.
TI Mean Element Propagations Using Numerical Averaging
SO JOURNAL OF THE ASTRONAUTICAL SCIENCES
LA English
DT Article
DE Averaging; Mean Elements; Orbits; Nonlinear Dynamics
AB The long-term evolution characteristics and stability of an orbit are well characterized using a mean element propagation of the perturbed two body variational equations of motion. The averaging process eliminates short period terms leaving only secular and long period effects. In this study, a non-traditional approach is taken that averages the variational equations using adaptive numerical techniques and then numerically integrating the resulting equations of motion. Doing this avoids the Fourier series expansions and truncations required by the traditional analytic methods. The resultant numerical techniques can be easily adapted to propagations at most solar system bodies.
C1 [Ely, Todd A.] CALTECH, Jet Prop Lab, Miss Design & Nav Sect, MS 301-121,4800 Oak Grove Dr, Pasadena, CA USA.
RP Ely, TA (reprint author), CALTECH, Jet Prop Lab, Miss Design & Nav Sect, MS 301-121,4800 Oak Grove Dr, Pasadena, CA USA.
EM Todd.A.Ely@jpl.nasa.gov
FU National Aeronautics and Space Administration
FX This work was carried out in part at the Jet Propulsion Laboratory,
California Institute of Technology, under contract with the National
Aeronautics and Space Administration.
NR 37
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U1 1
U2 1
PU AMER ASTRONAUTICAL SOC
PI SPRINGFIELD
PA 6352 ROLLING MILL PLACE SUITE 102, SPRINGFIELD, VA 22152 USA
SN 0021-9142
EI 2195-0571
J9 J ASTRONAUT SCI
JI J. Astronaut. Sci.
PD SEP
PY 2014
VL 61
IS 3
BP 275
EP 304
DI 10.1007/s40295-014-0020-2
PG 30
WC Engineering, Aerospace
SC Engineering
GA V41VZ
UT WOS:000209575000003
ER
PT J
AU Reuveni, Y
Kedar, S
Moore, A
Webb, F
AF Reuveni, Yuval
Kedar, Sharon
Moore, Angelyn
Webb, Frank
TI Analyzing slip events along the Cascadia margin using an improved
subdaily GPS analysis strategy
SO GEOPHYSICAL JOURNAL INTERNATIONAL
LA English
DT Article
DE Satellite geodesy; Transient deformation
ID SUBDUCTION ZONE; EPISODIC TREMOR; SILENT SLIP; SLOW; EARTHQUAKE;
INTERFACE; JAPAN; MODEL
AB A GPS analysis strategy that reduces the noise level of GPS-based subdaily strain measurements and improves subdaily resolution of positions enables the use of baseline estimates in the study of slow slip events along the northern Cascadia margin. We first evaluate this strategy's performance through comparisons of strain estimates at co-located GPS stations and borehole strainmetres, and then examine the strain migration during the 2008 May episodic tremor and slip (ETS) event. The temporal evolution of the ETS event is extracted from the GPS baseline analysis of the bidirectional propagation of the 2008 May event. These results establish the strain estimates from subdaily GPS baseline measurements as a reliable technique that can be used for mapping regional strain variations during episodic slip in regions where no laser or borehole strainmetres exist and GPS stations are abundant.
C1 [Reuveni, Yuval; Kedar, Sharon; Moore, Angelyn; Webb, Frank] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Reuveni, Y (reprint author), Univ Calif San Diego, Scripps Inst Oceanog, Inst Geophys & Planetary Phys, La Jolla, CA 92093 USA.
EM yreuveni@ucsd.edu
RI Reuveni, Yuval/J-8287-2015
FU National Aeronautics and Space Administration
FX The research was carried out at the Jet Propulsion Laboratory,
California Institute of Technology, under a contract with the National
Aeronautics and Space Administration. (C) 2012 California Institute of
Technology. Government sponsorship acknowledged. We would like to thank
Dr Susan Owen from Jet Propulsion Laboratory, California Institute of
Technology, for her suggestions and comments. We would also like to
thank Dr Herb Dragert from the Pacific Geo-science Center, Geological
Survey of Canada, for his assistance with GPS data. BSM data were
obtained from the PBO archives at
UNAVCO-ftp://bsm.unavco.org/pub/bsm/level2/.
NR 31
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U1 0
U2 15
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 SEP
PY 2014
VL 198
IS 3
BP 1269
EP 1278
DI 10.1093/gji/ggu208
PG 10
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA AM6EN
UT WOS:000339955900001
ER
PT J
AU Mousis, O
Choukroun, M
Lunine, JI
Sotin, C
AF Mousis, Olivier
Choukroun, Mathieu
Lunine, Jonathan I.
Sotin, Christophe
TI Equilibrium composition between liquid and clathrate reservoirs on Titan
SO ICARUS
LA English
DT Article
DE Titan; Titan, hydrology; Titan, surface; Titan, atmosphere
ID VAPOR-PRESSURE; DISSOCIATION PRESSURES; CHEMICAL-COMPOSITION;
NOBLE-GASES; STRUCTURE-I; METHANE; ETHANE; LAKES; ATMOSPHERE; NITROGEN
AB Hundreds of lakes and a few seas of liquid hydrocarbons have been observed by the Cassini spacecraft to cover the polar regions of Titan. A significant fraction of these lakes or seas could possibly be interconnected with subsurface liquid reservoirs of alkanes. In this paper, we investigate the interplay that would happen between a reservoir of liquid hydrocarbons located in Titan's subsurface and a hypothetical clathrate reservoir that progressively forms if the liquid mixture diffuses throughout a preexisting porous icy layer. To do so, we use a statistical-thermodynamic model in order to compute the composition of the clathrate reservoir that forms as a result of the progressive entrapping of the liquid mixture. This study shows that clathrate formation strongly fractionates the molecules between the liquid and the solid phases. Depending on whether the structures I or II clathrate forms, the present model predicts that the liquid reservoirs would be mainly composed of either propane or ethane, respectively. The other molecules present in the liquid are trapped in clathrates. Any river or lake emanating from subsurface liquid reservoirs that significantly interacted with clathrate reservoirs should present such composition. On the other hand, lakes and rivers sourced by precipitation should contain higher fractions of methane and nitrogen, as well as minor traces of argon and carbon monoxide. (C) 2014 Elsevier Inc. All rights reserved.
C1 [Mousis, Olivier] Univ Franche Comte, Inst UTINAM, UMR 6213, CNRS INSU, F-25030 Besancon, France.
[Mousis, Olivier; Lunine, Jonathan I.] Cornell Univ, Ctr Radiophys & Space Res, Ithaca, NY 14853 USA.
[Choukroun, Mathieu; Sotin, Christophe] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Mousis, O (reprint author), Univ Franche Comte, Inst UTINAM, UMR 6213, CNRS INSU, F-25030 Besancon, France.
EM olivier.mousis@obs-besancon.fr
RI Choukroun, Mathieu/F-3146-2017
OI Choukroun, Mathieu/0000-0001-7447-9139
FU CNES; NASA Outer Planets Research Program; Jet Propulsion Laboratory,
California Institute of Technology, under NASA
FX O.M. acknowledges support from CNES. M.C. and C.S. acknowledge support
from the NASA Outer Planets Research Program. Part of this work has been
conducted at the Jet Propulsion Laboratory, California Institute of
Technology, under contract to NASA. Government sponsorship acknowledged.
NR 40
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U1 0
U2 22
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 SEP 1
PY 2014
VL 239
BP 39
EP 45
DI 10.1016/j.icarus.2014.05.032
PG 7
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AM3WE
UT WOS:000339782700005
ER
PT J
AU O'Brien, DP
Walsh, KJ
Morbidelli, A
Raymond, SN
Mandell, AM
AF O'Brien, David P.
Walsh, Kevin J.
Morbidelli, Alessandro
Raymond, Sean N.
Mandell, Avi M.
TI Water delivery and giant impacts in the 'Grand Tack' scenario
SO ICARUS
LA English
DT Article
DE Planetary formation; Planetary dynamics; Planets, migration
ID TERRESTRIAL PLANET FORMATION; GASEOUS PROTOPLANETARY DISK;
HIGH-RESOLUTION SIMULATIONS; EARTH-LIKE PLANETS; ASTEROID BELT; HEAVY
BOMBARDMENT; PRIMORDIAL EXCITATION; SIDEROPHILE ELEMENTS; OLIGARCHIC
GROWTH; FORMING IMPACT
AB A new model for terrestrial planet formation (Hansen [2009]. Astrophys. J., 703, 1131-1140; Walsh, KJ., et al. [2011]. Nature, 2011, 206-209) has explored accretion in a truncated protoplanetary disk, and found that such a configuration is able to reproduce the distribution of mass among the planets in the Solar System, especially the Earth/Mars mass ratio, which earlier simulations have generally not been able to match. Walsh et al. (Walsh, KJ., et al. [2011]. Nature, 2011,206-209) tested a possible mechanism to truncate the disk a two-stage, inward-then-outward migration of Jupiter and Saturn, as found in numerous hydrodynamical simulations of giant planet formation. In addition to truncating the disk and producing a more realistic Earth/Mars mass ratio, the migration of the giant planets also populates the asteroid belt with two distinct populations of bodies the inner belt is filled by bodies originating inside of 3 AU, and the outer belt is filled with bodies originating from between and beyond the giant planets (which are hereafter referred to as 'primitive' bodies).
One implication of the truncation mechanism proposed in Walsh et al. (Walsh, KJ., et al. [2011]. Nature, 2011, 206-209) is the scattering of primitive planetesimals onto planet-crossing orbits during the formation of the planets. We find here that the planets will accrete on order 1-2% of their total mass from these bodies. For an assumed value of 10% for the water mass fraction of the primitive planetesimals, this model delivers a total amount of water comparable to that estimated to be on the Earth today. The radial distribution of the planetary masses and the dynamical excitation of their orbits are a good match to the observed system. However, we find that a truncated disk leads to formation timescales more rapid than suggested by radiometric chronometers. In particular, the last giant impact is typically earlier than 20 Myr, and a substantial amount of mass is accreted after that event. This is at odds with the dating of the Moon-forming impact and the estimated amount of mass accreted by Earth following that event. However, 5 of the 27 planets larger than half an Earth mass formed in all simulations do experience large late impacts and subsequent accretion consistent with those constraints. (C) 2014 The Authors. Published by Elsevier Inc. This is an open access article under the CC BY license
C1 [O'Brien, David P.] Planetmy Sci Inst, Tucson, AZ 85719 USA.
[Walsh, Kevin J.] SW Res Inst, Dept Space Studies, Boulder, CO 80302 USA.
[Morbidelli, Alessandro] Univ Nice Sophia Antipolis, CNRS, Observ Cote Azur, F-06304 Nice 4, France.
[Raymond, Sean N.] Univ Bordeaux, Observ Aquitain Sci Univers, F-33270 Floirac, France.
[Raymond, Sean N.] CNRS, UMR 5804, Lab Astrophys Bordeaux, F-33270 Floirac, France.
[Mandell, Avi M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP O'Brien, DP (reprint author), Planetmy Sci Inst, 1700 E Ft Lowell,Suite 106, Tucson, AZ 85719 USA.
EM obrien@psi.edu
FU NASA's Planetary Geology and Geophysics research program [NNX09AE36G];
NASA Lunar Science Institute (Center for Lunar Origin and Evolution at
the Southwest Research Institute in Boulder, Colorado); NASA
[NNA09DB32A]; European Research Council (ERC) [290568]
FX D.P. O'Brien was supported by Grant NNX09AE36G from NASA's Planetary
Geology and Geophysics research program. K.J. Walsh was supported by the
NASA Lunar Science Institute (Center for Lunar Origin and Evolution at
the Southwest Research Institute in Boulder, Colorado), NASA Grant
NNA09DB32A. D.P. O'Brien and A. Morbidelli acknowledge European Research
Council (ERC) Advanced Grant "ACCRETE" for support (contract Number
290568). We thank the two reviewers for their helpful comments and
suggestions.
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SN 0019-1035
EI 1090-2643
J9 ICARUS
JI Icarus
PD SEP 1
PY 2014
VL 239
BP 74
EP 84
DI 10.1016/j.icarus.2014.05.009
PG 11
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AM3WE
UT WOS:000339782700007
ER
PT J
AU Rubincam, DP
AF Rubincam, David Parry
TI The thermal expansion of particles and their secular orbital evolution
as they circle a planet
SO ICARUS
LA English
DT Article
DE Planetary rings; Celestial mechanics; Near-Earth objects; Mars,
satellites; zodiacal light
ID RADIATION PRESSURE; SOLAR-SYSTEM; RING; ASTEROIDS; TEMPERATURE; FORCES;
BODIES; EARTH
AB The thermal expansion and contraction of particles orbiting a planet can cause secular orbit evolution. This effect, called here the thermal expansion effect, depends on particles entering and exiting the shadow of the body they orbit. A particle cools off in the shadow and heats up again in the sunshine, suffering thermal contraction and expansion. The changing cross-section that the particle presents to solar radiation pressure, plus a time lag due to thermal inertia, lead to a net along-track force. The effect causes outward drift for rocky particles in circular orbits. For particles in the size range similar to 0.002-0.02 m orbiting the inner planets, particle orbits can outwardly evolve at the rate of similar to 0.1R(Plan) per million years for Mars to similar to 1R(Plan) per million years for Mercury for distances similar to 2R(Plan) from the body, where R-Plan is the planet's radius. Poynting-Robertson dominates thermal expansion beyond a few R-Plan for the inner planets. Hence there are distances from a planet where the effects balance, depending on particle size. Orbits evolving outward from the thermal expansion effect would stop there, as well as those inwardly evolving from Poynting-Robertson. Thus particles would accumulate in these places, assuming the absence of other forces. Mars appears to be the best candidate for the operation of the thermal expansion effect. Particles in the size range considered here and orbiting in the Phobos-Deimos region would tend to be collected by the moons, sweeping the particles up and perhaps helping keep the region free of dust. The thermal expansion effect is overwhelmed by Poynting-Robertson for rocky particles orbiting Jupiter and Saturn and thus is unimportant; these planets are not considered here. For particles orbiting small asteroids, the thermal expansion effect is much larger than the Poynting-Robertson effect, but both are overwhelmed by ordinary solar radiation pressure, which increases orbital eccentricities rapidly. Meteoroids in eccentric orbits about the Sun also suffer the thermal expansion effect, but with only similar to 0.0003e(2) AU change in semimajor axis over a million years for a 2 m meteoroid orbiting between Mercury and Earth. Published by Elsevier Inc.
C1 NASA, Goddard Space Flight Ctr, Planetary Geodynam Lab, Solar Syst Explorat Div, Greenbelt, MD 20771 USA.
RP Rubincam, DP (reprint author), NASA, Goddard Space Flight Ctr, Planetary Geodynam Lab, Solar Syst Explorat Div, Code 698,Bldg 34,Room S280, Greenbelt, MD 20771 USA.
EM David.P.Rubincam@nasa.gov
FU AES; SALMON
FX I thank Susan Fricke for excellent programming support, and David D.
Rowlands for making the GEODYN runs. I thank Stuart Pilorz and Daniel
Scheeres for valuable comments which greatly improved the paper. The
support of the AES and SALMON proposals is gratefully acknowledged.
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SN 0019-1035
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JI Icarus
PD SEP 1
PY 2014
VL 239
BP 96
EP 104
DI 10.1016/j.icarus.2014.05.025
PG 9
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AM3WE
UT WOS:000339782700009
ER
PT J
AU Neish, CD
Madden, J
Carter, LM
Hawke, BR
Giguere, T
Bray, VJ
Osinski, GR
Cahill, JTS
AF Neish, C. D.
Madden, J.
Carter, L. M.
Hawke, B. R.
Giguere, T.
Bray, V. J.
Osinski, G. R.
Cahill, J. T. S.
TI Global distribution of lunar impact melt flows
SO ICARUS
LA English
DT Article
DE Impact processes; Cratering; Moon; Moon, surface
ID OBLIQUE IMPACTS; MOON; CRATERS; RADAR; INSTRUMENT; EJECTA
AB In this study, we analyzed the distribution and properties of 146 craters with impact melt deposits exterior to their rims. Many of these craters were only recently discovered due to their unusual radar properties in the near-global Mini-RF data set. We find that most craters with exterior deposits of impact melt are small <= 20 km, and that the smallest craters have the longest melt flows relative to their size. In addition, exterior deposits of impact melt are more common in the highlands than the mare. This may be the result of differing target properties in the highlands and mare, the difference in titanium content, or the greater variation of topography in the highlands. We find that 80% of complex craters and 60% of simple craters have melt directions that are coincident or nearly coincident with the lowest point in their rim, implying that pre-existing topography plays a dominant role in melt emplacement. This is likely due to movement during crater modification (complex craters) or breached crater rims (simple craters). We also find that impact melt flows have very high circular polarization ratios compared to other features on the Moon. This suggests that their surfaces are some of the roughest material on the Moon at the centimeter to decimeter scale, even though they appear smooth at the meter scale. (C) 2014 Elsevier Inc. All rights reserved.
C1 [Neish, C. D.] Florida Inst Technol, Dept Phys & Space Sci, Melbourne, FL 32901 USA.
[Madden, J.] Franklin & Marshall Coll, Lancaster, PA 17603 USA.
[Carter, L. M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Hawke, B. R.; Giguere, T.] Univ Hawaii Manoa, Honolulu, HI 96822 USA.
[Giguere, T.] Intergraph Corp, Kapolei, HI 96707 USA.
[Bray, V. J.] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA.
[Osinski, G. R.] Univ Western Ontario, Dept Earth Sci, Ctr Planetary Sci & Explorat, London, ON N6A 3K7, Canada.
[Osinski, G. R.] Univ Western Ontario, Dept Phys & Astron, Ctr Planetary Sci & Explorat, London, ON N6A 3K7, Canada.
[Cahill, J. T. S.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA.
RP Neish, CD (reprint author), Florida Inst Technol, Dept Phys & Space Sci, Melbourne, FL 32901 USA.
EM cneish@fit.edu
RI Carter, Lynn/D-2937-2012; Cahill, Joshua/I-3656-2012;
OI Cahill, Joshua/0000-0001-6874-5533; Madden, Jack/0000-0002-4701-7833
FU NASA Postdoctoral Program at the Goddard Space Flight Center
FX We thank the LRO project for their effort in returning the data
presented here. We also wish to thank Bruce Campbell and Lillian Ostrach
for their careful reviews, and Natalie Glines for help in the early
stages of this work. This work was supported in part 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.
NR 53
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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 SEP 1
PY 2014
VL 239
BP 105
EP 117
DI 10.1016/j.icarus.2014.05.049
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AM3WE
UT WOS:000339782700010
ER
PT J
AU Lee, S
Hofstadter, M
Frerking, MA
Gulkis, S
von Allmen, P
Crovisier, J
Biver, N
Bockelee-Morvan, D
Kamp, L
Choukroun, M
Keihm, S
Janssen, M
AF Lee, Seungwon
Hofstadter, Mark
Frerking, Margaret A.
Gulkis, Samuel
von Allmen, Paul
Crovisier, Jacques
Biver, Nicolas
Bockelee-Morvan, Dominique
Kamp, Lucas
Choukroun, Mathieu
Keihm, Stephen
Janssen, Michael
TI Sub-millimeter observation of water vapor at 557 GHz in Comet C/2002 T7
(LINEAR)
SO ICARUS
LA English
DT Article
DE Comets, coma; Radio observations; Comets, composition
ID RADIATIVE-TRANSFER; NUCLEI; NEAT; Q4; 67P/CHURYUMOV-GERASIMENKO;
WAVELENGTHS; INSTRUMENT; SIMULATION; MILLIMETER; ROTATION
AB We present sub-millimeter observations of the ground-state rotational transition (1(10)-1(01)) of water vapor from Comet C/2002 T7 (LINEAR) obtained with the MIRO instrument on the ESA Rosetta spacecraft (s/c) orbiter on April 30, 2004. At the time of the observations, the comet was at a distance of 0.63 AU from the Sun, 0.68 AU from the MIRO telescope, and about 7.5 days after its perihelion. The ground state rotation transition of ortho-water at 556.936 GHz was observed and integrated for similar to 8 h using a frequency switched radiometer to provide short and long term stability. The MIRO beam size is 7.5 arcmin in terms of full width half maximum, corresponding to a radius of 1.1 x 10(5) km at the comet location. The observed signal line area of the water line spectrum is 4.3 +/- 0.8 K km/s. Using a molecular excitation and radiation transfer model and assuming the spherically symmetric and constant radial expansion of gas in the coma, we estimate that the production rate of water is (1.0 +/- 0.2) x 10(30) molecules/s and the expansion velocity is 1.1 +/- 0.2 km/s at the time of the MIRO observation. The present estimation of the water outgassing rate of the comet is in good agreement with other observation-based estimations when the outgassing rates with respect to the time after perihelion are compared. The Doppler-corrected center velocity of the observed line was red-shifted by 0.67 +/- 0.13 km/s, of which only 0.18 km/s shift is explained by the model and attributed to a self-absorption effect. The potential sources of the additional red shift are discussed. Published by Elsevier Inc.
C1 [Lee, Seungwon; Hofstadter, Mark; Frerking, Margaret A.; Gulkis, Samuel; von Allmen, Paul] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Crovisier, Jacques; Biver, Nicolas; Bockelee-Morvan, Dominique; Kamp, Lucas; Choukroun, Mathieu; Keihm, Stephen; Janssen, Michael] Univ Paris Diderot, UPMC, CNRS, LESIA,Observ Paris, F-92195 Meudon, France.
RP Lee, S (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM seungwon.lee@jpl.nasa.gov
RI Choukroun, Mathieu/F-3146-2017
OI Choukroun, Mathieu/0000-0001-7447-9139
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PI SAN DIEGO
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SN 0019-1035
EI 1090-2643
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JI Icarus
PD SEP 1
PY 2014
VL 239
BP 141
EP 153
DI 10.1016/j.icarus.2014.05.004
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AM3WE
UT WOS:000339782700013
ER
PT J
AU Schroder, SE
Grynko, Y
Pommerol, A
Keller, HU
Thomas, N
Roush, TL
AF Schroeder, S. E.
Grynko, Ye.
Pommerol, A.
Keller, H. U.
Thomas, N.
Roush, T. L.
TI Laboratory observations and simulations of phase reddening
SO ICARUS
LA English
DT Article
DE Spectrophotometry; Regoliths; Mineralogy; Radiative transfer
ID BIDIRECTIONAL REFLECTANCE SPECTROSCOPY; DAWN FRAMING CAMERA; OPTICS
APPROXIMATION; LIGHT-SCATTERING; LUNAR-SURFACE; SEMITRANSPARENT
PARTICLES; PHOTOMETRIC PROPERTIES; WAVELENGTH DEPENDENCE; SPECTRAL
REFLECTANCE; PARTICULATE SURFACES
AB The visible reflectance spectrum of many Solar System bodies changes with changing viewing geometry for reasons not fully understood. It is often observed to redden (increasing spectral slope) with increasing solar phase angle, an effect known as phase reddening. Only once, in an observation of the martian surface by the Viking 1 lander, was reddening observed up to a certain phase angle with bluing beyond, making the reflectance ratio as a function of phase angle shaped like an arch. However, in laboratory experiments this arch-shape is frequently encountered. To investigate this, we measured the bidirectional reflectance of particulate samples of several common rock types in the 400-1000 nm wavelength range and performed ray-tracing simulations. We confirm the occurrence of the arch for surfaces that are forward scattering, i.e. are composed of semi-transparent particles and are smooth on the scale of the particles, and for which the reflectance increases from the lower to the higher wavelength in the reflectance ratio. The arch shape is reproduced by the simulations, which assume a smooth surface. However, surface roughness on the scale of the particles, such as the Hapke and van Horn (Hapke, B., van Horn, H. [1963]. J. Geophys. Res. 68, 4545-4570) fairy castles that can spontaneously form when sprinkling a fine powder, leads to monotonic reddening. A further consequence of this form of microscopic roughness (being indistinct without the use of a microscope) is a flattening of the disk function at visible wavelengths, i.e. Lommel-Seeliger-type scattering. The experiments further reveal monotonic reddening for reflectance ratios at near-IR wavelengths. The simulations fail to reproduce this particular reddening, and we suspect that it results from roughness on the surface of the particles. Given that the regolith of atmosphereless Solar System bodies is composed of small particles, our results indicate that the prevalence of monotonic reddening and Lommel Seeliger-type scattering for these bodies results from microscopic roughness, both in the form of structures built by the particles and roughness on the surface of the particles themselves. It follows from the singular Viking 1 observation that the surface in front of the Lander was composed of semi-transparent particles, and was smooth on the scale of the particle size. (C) 2014 Elsevier Inc. All rights reserved.
C1 [Schroeder, S. E.] Deutsch Zentrum Luft & Raumfahrt DLR, D-12489 Berlin, Germany.
[Grynko, Ye.] Univ Paderborn, D-33098 Paderborn, Germany.
[Pommerol, A.; Thomas, N.] Univ Bern, Inst Phys, CH-3012 Bern, Switzerland.
[Keller, H. U.] Tech Univ Carolo Wilhelmina Braunschweig, Inst Geophys & Extraterr Phys IGEP, D-38106 Braunschweig, Germany.
[Roush, T. L.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
RP Schroder, SE (reprint author), Deutsch Zentrum Luft & Raumfahrt DLR, D-12489 Berlin, Germany.
EM stefanus.schroeder@dlr.de
RI Schroder, Stefan/D-9709-2013
OI Schroder, Stefan/0000-0003-0323-8324
FU Swiss National Science Foundation
FX We are grateful to Lyuba Moroz for her help in procuring the samples and
Ines Buttner for her assistance in preparing the samples. Fred Goesmann
kindly allowed the first author to use his scanning electron microscope.
Comments by reviewers J.R. Johnson and Y. Shkuratov helped to improve
the manuscript. S.E.S. thanks Stefano Mottola for fruitful discussions
and reviewing the draft paper. Development of the PHIRE goniometer has
been supported by the Swiss National Science Foundation.
NR 64
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PI SAN DIEGO
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SN 0019-1035
EI 1090-2643
J9 ICARUS
JI Icarus
PD SEP 1
PY 2014
VL 239
BP 201
EP 216
DI 10.1016/j.icarus.2014.06.010
PG 16
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AM3WE
UT WOS:000339782700018
ER
PT J
AU Farrell, WM
Wahlund, JE
Morooka, M
Gurnett, DA
Kurth, WS
MacDowall, RJ
AF Farrell, W. M.
Wahlund, J-E
Morooka, M.
Gurnett, D. A.
Kurth, W. S.
MacDowall, R. J.
TI An estimate of the dust pickup current at Enceladus
SO ICARUS
LA English
DT Article
DE Saturn; Enceladus; Satellites, general
ID SOUTH-POLE; PLASMA; ATMOSPHERE; RADIO; PLUME
AB We demonstrate that the acceleration of submicron dust originating at Enceladus by a reduced co-rotating E-field is capable of creating a dust pickup current perpendicular to the magnetic field with values ranging from 3 to 15 kA (depending upon the effective grain charge). Such a current represents a new contribution to the total pickup current in the region. As such, we suggest that dust pickup currents, along with ion and electron pickup currents, are all active within the plume. Published by Elsevier Inc.
C1 [Farrell, W. M.; MacDowall, R. J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Wahlund, J-E; Morooka, M.] Swedish Inst Space Phys, Uppsala, Sweden.
[Gurnett, D. A.; Kurth, W. S.] Univ Iowa, Iowa City, IA 52242 USA.
RP Farrell, WM (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
EM william.m.farrell@nasa.gov
RI Farrell, William/I-4865-2013;
OI Kurth, William/0000-0002-5471-6202
NR 28
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VL 239
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EP 221
DI 10.1016/j.icarus.2014.05.034
PG 5
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AM3WE
UT WOS:000339782700019
ER
PT J
AU Nathues, A
Hoffmann, M
Cloutis, EA
Schafer, M
Reddy, V
Christensen, U
Sierks, H
Thangjam, GS
Le Corre, L
Mengel, K
Vincent, JB
Russell, CT
Prettyman, T
Schmedemann, N
Kneissl, T
Raymond, C
Gutierrez-Marques, P
Hall, I
Buttner, I
AF Nathues, Andreas
Hoffmann, Martin
Cloutis, Edward A.
Schaefer, Michael
Reddy, Vishnu
Christensen, Ulrich
Sierks, Holger
Thangjam, Guneshwar Singh
Le Corre, Lucille
Mengel, Kurt
Vincent, Jean-Baptist
Russell, Christopher T.
Prettyman, Tom
Schmedemann, Nico
Kneissl, Thomas
Raymond, Carol
Gutierrez-Marques, Pablo
Hall, Ian
Buettner, Irene
TI Detection of serpentine in exogenic carbonaceous chondrite material on
Vesta from Dawn FC data
SO ICARUS
LA English
DT Article
DE Asteroid Vesta; Asteroids, composition; Mineralogy; Spectroscopy
ID SPECTRAL REFLECTANCE PROPERTIES; ASTEROID 4 VESTA; HED METEORITES; CM
CHONDRITES; DARK MATERIAL; GRAIN-SIZE; MAIN-BELT; MINERALS;
SPECTROSCOPY; HOWARDITES
AB The Dawn mission's Framing Camera (FC) observed Asteroid (4) Vesta in 2011 and 2012 using seven color filters and one clear filter from different orbits. In the present paper we analyze recalibrated HAMO color cubes (spatial resolution similar to 60 m/pixel) with a focus on dark material (DM). We present a definition of highly concentrated DM based on spectral parameters, subsequently map the DM across the Vestan surface, geologically classify DM, study its spectral properties on global and local scales, and finally, compare the FC in-flight color data with laboratory spectra.
We have discovered an absorption band centered at 0.72 mu m in localities of DM that show the lowest albedo values by using FC data as well as spectral information from Dawn's imaging spectrometer VIR. Such localities are contained within impact-exposed outcrops on inner crater walls and ejecta material. Comparisons between spectral FC in-flight data, and laboratory spectra of meteorites and mineral mixtures in the wavelength range 0.4-1.0 mu m, revealed that the absorption band can be attributed to the mineral serpentine, which is typically present in CM chondrites. Dark material in its purest form is rare on Vesta's surface and is distributed globally in a non-uniform manner. Our findings confirm the hypothesis of an exogenic origin of the DM by the infall of carbonaceous chondritic material, likely of CM type. It further confirms the hypothesis that most of the DM was deposited by the Veneneia impact. (C) 2014 Elsevier Inc. All rights reserved.
C1 [Nathues, Andreas; Hoffmann, Martin; Schaefer, Michael; Reddy, Vishnu; Christensen, Ulrich; Sierks, Holger; Thangjam, Guneshwar Singh; Vincent, Jean-Baptist; Gutierrez-Marques, Pablo; Hall, Ian; Buettner, Irene] Max Planck Inst Solar Syst Res, D-37077 Gottingen, Germany.
[Cloutis, Edward A.] Univ Winnipeg, Dept Geog, Winnipeg, MB R3B 2E9, Canada.
[Reddy, Vishnu; Le Corre, Lucille; Prettyman, Tom] Planetary Sci Inst, Tucson, AZ 85719 USA.
[Mengel, Kurt] Tech Univ Clausthal, D-38678 Clausthal Zellerfeld, Germany.
[Russell, Christopher T.] Univ Calif Los Angeles, Inst Geophys & Planetary Phys, Los Angeles, CA 90095 USA.
[Raymond, Carol] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Schmedemann, Nico; Kneissl, Thomas] Free Univ Berlin, Berlin, Germany.
RP Nathues, A (reprint author), Max Planck Inst Solar Syst Res, Justus von Liebig Weg 3, D-37077 Gottingen, Germany.
EM nathues@mps.mpg.de
OI Reddy, Vishnu/0000-0002-7743-3491; Prettyman,
Thomas/0000-0003-0072-2831; Le Corre, Lucille/0000-0003-0349-7932
FU Max Planck Society; DLR; NASA/JPL
FX The authors would like to thank the Dawn Flight Operations team for a
successful Vesta phase. AN would like to thank MPS, DLR and IDA
colleagues which worked hard to design, built and test the Framing
Cameras. The camera system was developed and built under the leadership
of the Max-Planck-Institute for Solar System Research. The Institute for
Planetary Research of the German Space Agency DLR provided the Front End
Electronics as well as the CCD. The Institute of Computer and
Communication Network Engineering provided the main electronics of the
cameras. The project is financially supported by the Max Planck Society,
DLR, and NASA/JPL.
NR 79
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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
EI 1090-2643
J9 ICARUS
JI Icarus
PD SEP 1
PY 2014
VL 239
BP 222
EP 237
DI 10.1016/j.icarus.2014.06.003
PG 16
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AM3WE
UT WOS:000339782700020
ER
PT J
AU Kim, JR
Schumann, G
Neal, JC
Lin, SY
AF Kim, Jung-Rack
Schumann, Guy
Neal, Jeffrey C.
Lin, Shih-Yuan
TI Megaflood analysis through channel networks of the Athabasca Valles,
Mars based on multi-resolution stereo DTMs and 2D hydrodynamic modeling
SO PLANETARY AND SPACE SCIENCE
LA English
DT Article
DE DTM; Hydraulic model; Mars; Stereo analysis; Water flow
ID ORBITER LASER ALTIMETER; DIGITAL TERRAIN MODELS; CERBERUS FOSSAE; LAVA;
GROUNDWATER; EMPLACEMENT; DEPOSITS; ELYSIUM; EQUATOR; SURFACE
AB Stereo analysis of in-orbital imagery provides valuable topographic data for scientific research over planetary surfaces especially for the interpretation of potential fluvial activity. The focus of research into planetary fluvial activity has been shifting toward quantitative modeling with various spatial resolution DTMs from visual interpretation with ortho images. Thus in this study, we tested the application of hydraulic analysis with multi resolution Martian DTMs, which were constructed following the approaches of Kim and Muller (2009). Planet. Space Sci. 57 (14), 2095. Subsequently, a two-dimensional hydraulic model was introduced to conduct flow simulation using the extracted 1.2-150 m resolution DTMs. As a result, it was found that the simulated water flows coincided with what might be water eroded geomorphic features over target areas. Moreover, the information acquired from the modeling, such as water depth along the time line, flow direction and travel time, is proving of great value for the interpretation of surface characteristics. Results highlighted the importance of DTM quality for simulating fluvial channel hydraulics across planetary surfaces. (C) 2014 Elsevier Ltd. All rights reserved.
C1 [Kim, Jung-Rack] Univ Seoul, Dept Geoinformat, Seoul 130743, South Korea.
[Schumann, Guy] CALTECH, NASA, Jet Prop Lab, Pasadena, CA USA.
[Neal, Jeffrey C.] Univ Bristol, Sch Geog Sci, Bristol, Avon, England.
[Lin, Shih-Yuan] Natl Chengchi Univ, Dept Land Econ, Taipei 11623, Taiwan.
RP Kim, JR (reprint author), Univ Seoul, Dept Geoinformat, 163 Seoulsiripdaero, Seoul 130743, South Korea.
EM kjrr001@gmail.com
RI Schumann, Guy/F-9760-2011
FU National Research Foundation of Korea [2013078206]; National Aeronautics
and Space Administration
FX The authors would like to acknowledge the HRSC-CoI team, especially the
former PI, Prof. Gerhard Neukum and the HiRISE team for providing the
valuable data sets. The first author would like to thank National
Research Foundation of Korea for supporting this study (Grant no.
2013078206). Guy Schumann's time at the Jet Propulsion Laboratory,
California Institute of Technology was funded under a contract with the
National Aeronautics and Space Administration.
NR 50
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U1 0
U2 12
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 SEP
PY 2014
VL 99
BP 55
EP 69
DI 10.1016/j.pss.2014.04.010
PG 15
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AM2SA
UT WOS:000339699900007
ER
PT J
AU Szwarc, T
Hubbard, S
AF Szwarc, Timothy
Hubbard, Scott
TI Thermal mapping and trends of Mars analog materials in sample
acquisition operations using experimentation and models
SO PLANETARY AND SPACE SCIENCE
LA English
DT Article
DE Rotary-percussive; Coring; Drilling; Mars; Analog
ID STRENGTH; ROCK
AB The effects of atmosphere, ambient temperature, and geologic material were studied experimentally and using a computer model to predict the heating undergone by Mars rocks during rover sampling operations. Tests were performed on five well-characterized and/or Mars analog materials: Indiana limestone, Saddleback basalt, kaolinite, travertine, and water ice. Eighteen tests were conducted to 55 mm depth using a Mars Sample Return prototype coring drill, with each sample containing six thermal sensors. A thermal simulation was written to predict the complete thermal profile within each sample during coring and this model was shown to be capable of predicting temperature increases with an average error of about 7%. This model may be used to schedule power levels and periods of rest during actual sample acquisition processes to avoid damaging samples or freezing the bit into icy formations. Maximum rock temperature increase is found to be modeled by a power law incorporating rock and operational parameters. Energy transmission efficiency in coring is found to increase linearly with rock hardness and decrease by 31% at Mars pressure. (C) 2014 Elsevier Ltd. All rights reserved.
C1 [Szwarc, Timothy] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Hubbard, Scott] Stanford Univ, Dept Aeronaut & Astronaut, Stanford, CA 94305 USA.
RP Szwarc, T (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM timothy.j.szwarc@jpl.nasa.gov; scotthub@stanford.edu
FU JPL Strategic University research Partnership (SURP) [1481914]
FX This research was made possible by the financial support of the JPL
Strategic University research Partnership (SURP) (1481914). The authors
would like to thank Neil Murphy and Lori Shiraishi of JPL. Experimental
work was conducted at Honeybee Robotics Spacecraft Mechanisms
corporation in Pasadena, CA. In particular, the authors would like to
thank Dr. Kris Zacny and Gale Paulsen for their time and resources. The
authors would also like to thank Professor Brian Cantwell, Professor
Richard Christensen, and Professor David Pollard of Stanford University
for their input to the experimental test plan and analysis.
NR 12
TC 0
Z9 0
U1 2
U2 6
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 SEP
PY 2014
VL 99
BP 158
EP 166
DI 10.1016/j.pss.2014.06.002
PG 9
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AM2SA
UT WOS:000339699900016
ER
PT J
AU McGillivray, DA
Cravey, RL
Dudley, KL
Vedeler, E
Gupta, MC
AF McGillivray, Duncan A.
Cravey, Robin L.
Dudley, Kenneth L.
Vedeler, Erik
Gupta, Mool C.
TI POLARIZATION PROPERTIES OF A 2-D SPLIT RING RESONATOR AND ROD TYPE
METAMATERIAL LENS
SO MICROWAVE AND OPTICAL TECHNOLOGY LETTERS
LA English
DT Article
DE metamaterials; split ring resonators; polarization; transmission;
sensors; metamaterial lens
ID NEGATIVE REFRACTION
AB The polarization state of microwave (MW) radiation transmitted through a 2-D split ring resonator and rod metamaterial (MTM) lens is investigated. At a resonance frequency of 3.63 GHz, the 2-D lens modifies the polarization state of the incident radiation. For E-y incident polarization, the transmitted wave exhibits elliptical polarization as well as a tilt in the principal axis. The ellipticity is dependent on the incident polarization angle. A Ex polarized incident MW is unaffected. Transformation of polarization properties plays an important role for manipulation and control of MW radiation, impacting existing applications and providing opportunities for novel MTMs-based sensors and other applications. (C) 2014 Wiley Periodicals, Inc.
C1 [McGillivray, Duncan A.; Gupta, Mool C.] Univ Virginia, Dept Elect & Comp Engn, Charlottesville, VA 22904 USA.
[Cravey, Robin L.; Dudley, Kenneth L.; Vedeler, Erik] NASA, Langley Res Ctr, Electromagnet & Sensors Branch, Hampton, VA 23681 USA.
RP Gupta, MC (reprint author), Univ Virginia, Dept Elect & Comp Engn, Charlottesville, VA 22904 USA.
EM mgupta@virginia.edu
NR 16
TC 0
Z9 0
U1 2
U2 15
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 0895-2477
EI 1098-2760
J9 MICROW OPT TECHN LET
JI Microw. Opt. Technol. Lett.
PD SEP
PY 2014
VL 56
IS 9
BP 2146
EP 2150
DI 10.1002/mop.28547
PG 6
WC Engineering, Electrical & Electronic; Optics
SC Engineering; Optics
GA AL9DE
UT WOS:000339439000047
ER
PT J
AU Madni, AM
Sievers, M
AF Madni, Azad M.
Sievers, Michael
TI System of Systems Integration: Key Considerations and Challenges
SO SYSTEMS ENGINEERING
LA English
DT Article
DE system of systems; system of systems integration; human-systems
integration; interoperability; integration ontology
ID FUTURE
AB As systems are called on to participate on demand within system-of-systems (SoS), system-of-systems integration (SoSI) has become a key concern. This capability is especially important in defense and aerospace where systems are increasingly required to interoperate on demand to satisfy mission requirements. SoSI is also becoming increasingly important in healthcare and energy domains. SoSI involves interfacing and enabling the interactions of component systems to create the needed SoS capability to accomplish mission or business goals. SoSI, which is part of the overall SoS development life cycle, increases in complexity when there are legacy systems that need to be integrated, and when humans are tasked to perform in various capacities within the SoS. An added layer of complexity is introduced when the SoS has to exhibit certain quality attributes such as adaptability and resilience in the face of contingencies and disruptions in the operational environment. This paper addresses key considerations and challenges in SoSI. (C) 2013 Wiley Periodicals, Inc.
C1 [Madni, Azad M.] Univ So Calif, Daniel J Epstein Dept Ind & Syst Engn, Viterbi Sch Engn, Los Angeles, CA 90089 USA.
[Sievers, Michael] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Madni, AM (reprint author), Univ So Calif, Daniel J Epstein Dept Ind & Syst Engn, Viterbi Sch Engn, Los Angeles, CA 90089 USA.
EM azad.madni@usc.edu
NR 43
TC 6
Z9 6
U1 1
U2 25
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 1098-1241
EI 1520-6858
J9 SYSTEMS ENG
JI Syst. Eng.
PD FAL
PY 2014
VL 17
IS 3
BP 330
EP 347
DI 10.1002/sys.21272
PG 18
WC Engineering, Industrial; Operations Research & Management Science
SC Engineering; Operations Research & Management Science
GA AL8HG
UT WOS:000339378300006
ER
PT J
AU Weisbin, CR
Lincoln, W
Saatchi, S
AF Weisbin, Charles R.
Lincoln, William
Saatchi, Sassan
TI A Systems Engineering Approach to Estimating Uncertainty in Above-Ground
Biomass (AGB) Derived from Remote-Sensing Data
SO SYSTEMS ENGINEERING
LA English
DT Article
DE above-ground biomass (AGB); uncertainty; correlation of uncertainties;
remote sensing; carbon; carbon cycle; carbon monitoring; carbon
measurement; forests; risk reduction
ID RADAR BACKSCATTER; TROPICAL REGIONS; FOREST BIOMASS; CARBON STOCKS; SAR
DATA; DEFORESTATION; INVENTORY; EMISSIONS; LIDAR; MAP
AB We integrate systems of measurement and modeling to improve estimation of uncertainties in above-ground biomass (AGB) derived from remote sensing. The outcome provides a unified starting point for the climate-change carbon community to assess uncertainty and sensitivity data and methodologies, and ultimately supports decision-making about which missions and instruments to develop for a desired cost/benefit ratio. Initial results include fusion of remote-sensing techniques (e. g., radar and lidar), uncertainties associated with measurement and modeling, and the impact of potential uncertainty correlations across aggregated unit areas. Biomass uncertainty estimates are presented at the single-hectare level for the forestlands of California. Using a forest biomass map of California, we calculate changes in variance (e. g., 2 orders of magnitude) as a function of uncertainty correlation assumptions, with correlations extending to spatial scales up to 100 km. Using a variogram formalism to derive the correlation shape and magnitude, we show that the estimated variance for California above-ground biomass is between 1% and 2% (1 standard deviation) for our current best estimate of the correlation range at 5-10 km-i.e., we bound the standard deviation by a factor of 2. This contrasts with 0.025% (1 standard deviation) if one does not include the correlation term. (C) 2013 Wiley Periodicals, Inc.
C1 [Weisbin, Charles R.; Lincoln, William; Saatchi, Sassan] CALTECH, NASA Jet Prop Lab, Pasadena, CA 91109 USA.
RP Weisbin, CR (reprint author), CALTECH, NASA Jet Prop Lab, Pasadena, CA 91109 USA.
EM Charles.R.Weisbin@jpl.nasa.gov; William.Lincoln@jpl.nasa.gov;
Saatchi@jpl.nasa.gov
FU NASA under the Carbon Monitoring System study task within the NASA Earth
Science Program
FX NASA under the Carbon Monitoring System study task within the NASA Earth
Science Program.
NR 43
TC 1
Z9 1
U1 1
U2 17
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 1098-1241
EI 1520-6858
J9 SYSTEMS ENG
JI Syst. Eng.
PD FAL
PY 2014
VL 17
IS 3
BP 361
EP 373
DI 10.1002/sys.21275
PG 13
WC Engineering, Industrial; Operations Research & Management Science
SC Engineering; Operations Research & Management Science
GA AL8HG
UT WOS:000339378300008
ER
PT J
AU Guhathakurta, M
AF Guhathakurta, Madhulika
TI Preface
SO SOLAR PHYSICS
LA English
DT Editorial Material
C1 NASA Headquarters, Washington, DC 20546 USA.
RP Guhathakurta, M (reprint author), NASA Headquarters, Washington, DC 20546 USA.
EM madhulika.guhathakurta@nasa.gov
NR 17
TC 1
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U1 0
U2 1
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0038-0938
EI 1573-093X
J9 SOL PHYS
JI Sol. Phys.
PD SEP
PY 2014
VL 289
IS 9
BP 3231
EP 3232
DI 10.1007/s11207-014-0560-4
PG 2
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AL3AL
UT WOS:000338997200001
ER
PT J
AU Liu, W
Ofman, L
AF Liu, Wei
Ofman, Leon
TI Advances in Observing Various Coronal EUV Waves in the SDO Era and Their
Seismological Applications (Invited Review)
SO SOLAR PHYSICS
LA English
DT Article
DE Corona, structures; Coronal mass ejections, low coronal signatures;
Coronal seismology; Flares, waves; Waves, magnetohydrodynamic; Waves,
propagation
ID EXTREME-ULTRAVIOLET WAVE; KELVIN-HELMHOLTZ INSTABILITY; QUASI-PERIODIC
PULSATIONS; SOLAR ENERGETIC PARTICLES; MAGNETIC-FIELD STRENGTH; FAST
MAGNETOSONIC WAVES; 2011 FEBRUARY 15; EMISSION MEASURE DIAGNOSTICS;
IMAGING TELESCOPE WAVE; MICRO-SIGMOID ERUPTION
AB Global extreme-ultraviolet (EUV) waves are spectacular traveling disturbances in the solar corona associated with energetic eruptions such as coronal mass ejections (CMEs) and flares. Over the past 15 years, observations from three generations of space-borne EUV telescopes have shaped our understanding of this phenomenon and at the same time led to controversy about its physical nature. Since its launch in 2010, the Atmospheric Imaging Assembly (AIA) onboard the Solar Dynamics Observatory (SDO) has observed more than 210 global EUV waves in exquisite detail, thanks to its high spatio-temporal resolution and full-disk, wide-temperature coverage. A combination of statistical analysis of this large sample, more than 30 detailed case studies, and data-driven MHD modeling, has been leading their physical interpretations to a convergence, favoring a bimodal composition of an outer, fast-mode magnetosonic wave component and an inner, non-wave CME component. Adding to this multifaceted picture, AIA has also discovered new EUV wave and wave-like phenomena associated with various eruptions, including quasi-periodic fast propagating (QFP) wave trains, magnetic Kelvin-Helmholtz instabilities (KHI) in the corona and associated nonlinear waves, and a variety of mini-EUV waves. Seismological applications using such waves are now being actively pursued, especially for the global corona. We review such advances in EUV wave research focusing on recent SDO/AIA observations, their seismological applications, related data-analysis techniques, and numerical and analytical models.
C1 [Liu, Wei] Stanford Univ, WW Hansen Expt Phys Lab, Stanford, CA 94305 USA.
[Liu, Wei] Lockheed Martin Solar & Astrophys Lab, Palo Alto, CA 94304 USA.
[Ofman, Leon] Catholic Univ Amer, Greenbelt, MD 20771 USA.
[Ofman, Leon] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Ofman, Leon] Tel Aviv Univ, Dept Geophys & Planetary Sci, IL-69978 Tel Aviv, Israel.
RP Liu, W (reprint author), Lockheed Martin Solar & Astrophys Lab, Bldg 252,3251 Hanover St, Palo Alto, CA 94304 USA.
EM weiliu@lmsal.com; Leon.Ofman@nasa.gov
OI Liu, Wei/0000-0001-8794-3420
FU NASA Living With a Star (LWS) Program [NNX11AO68G]; NASA [NNX12AB34G]
FX This work is supported by the NASA Living With a Star (LWS) Program
(grant NNX11AO68G). Additional support to LO was provided by NASA grant
NNX12AB34G. Special thanks go to Barbara Thompson for inviting both
authors to the 2013 LWS SDO Science Workshop that led to this topical
issue and this review. We are grateful to the anonymous referee for
constructive comments and suggestions that helped improve this article.
WL thanks Nariaki Nitta, Cooper Downs, Barbara Thompson, Angelos
Vourlidas, Peng-Fei Chen, Spiros Patsourakos, and Kyoung-Sun Lee for
critical comments on the manuscript and/or fruitful discussions. We
thank Suli Ma, Alexander Warmuth, Nariaki Nitta, Ding Yuan, Ute Mostl
(now Ute Amerstorfer), Nat Gopalswamy, Jason Byrne, and David Pascoe for
providing the original figures, and especially Cooper Downs, Liheng
Yang, Ting Li, Eoin Carley, and Ryun-Young Kwon for customizing their
figures to fit the layout of this article. Figures 1c and 1d, 2, 3, 4
(right), 5, 6a, 6c, and 6i, 8, 9, 11 (middle and right), 12a, 13, 14,
15a-15c, and 16 (left and middle) are reproduced by permission of the
AAS. Figures 4 (left), 11 (left), 15 (right), and 16 (right) are
reproduced with permission from Astronomy & Astrophysics, (C) ESO.
NR 281
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U2 15
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0038-0938
EI 1573-093X
J9 SOL PHYS
JI Sol. Phys.
PD SEP
PY 2014
VL 289
IS 9
BP 3233
EP 3277
DI 10.1007/s11207-014-0528-4
PG 45
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AL3AL
UT WOS:000338997200002
ER
PT J
AU Young, PR
Muglach, K
AF Young, P. R.
Muglach, K.
TI Solar Dynamics Observatory and Hinode Observations of a Blowout Jet in a
Coronal Hole
SO SOLAR PHYSICS
LA English
DT Article
DE Coronal holes; Jets; Magnetic fields, photosphere; Spectral line,
intensity and diagnostics; Spectrum, ultraviolet; Velocity fields,
photosphere
ID X-RAY TELESCOPE; MAGNETIC-FIELD; IMAGING SPECTROMETER; ATOMIC DATABASE;
EMISSION-LINES; QUIET SUN; SDO; MISSION; BOUNDARIES; CHIANTI
AB A blowout jet occurred within the south coronal hole on 9 February 2011 at 09:00 UT and was observed by the Atmospheric Imaging Assembly (AIA) and Helioseismic and Magnetic Imager (HMI) onboard the Solar Dynamics Observatory, and by the EUV Imaging Spectrometer (EIS) and X-Ray Telescope (XRT) onboard the Hinode spacecraft during coronal-hole monitoring performed as part of Hinode Operations Program No. 177. Images from AIA show expanding hot and cold loops from a small bright point with plasma ejected in a curtain up to 30 Mm wide. The initial intensity front of the jet had a projected velocity of 200 km s(-1), and the line-of-sight (LOS) velocities measured by EIS are between 100 and 250 km s(-1). The LOS velocities increased along the jet, implying that an acceleration mechanism operates within the body of the jet. The jet plasma had a density of 2.7x10(8) cm(-3) and a temperature of 1.4 MK. During the event a number of bright kernels were seen at the base of the bright point. The kernels have sizes of a parts per thousand aEuro parts per thousand 1000 km, are variable in brightness, and have lifetimes of 1 -aEuro parts per thousand 15 minutes. An XRT filter ratio yields temperatures of 1.5 -aEuro parts per thousand 3.0 MK for the kernels. The bright point existed for at least ten hours, but disappeared within two hours after the jet, which lasted for 30 minutes. HMI data reveal converging photospheric flows at the location of the bright point, and the mixed-polarity magnetic flux canceled over a period of four hours on either side of the jet.
C1 [Young, P. R.] George Mason Univ, Coll Sci, Fairfax, VA 22030 USA.
[Muglach, K.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Muglach, K.] ARTEP Inc, Ellicott City, MD 21042 USA.
RP Young, PR (reprint author), George Mason Univ, Coll Sci, 4400 Univ Dr, Fairfax, VA 22030 USA.
EM pyoung9@gmu.edu; kmuglach@gmx.de
OI Young, Peter/0000-0001-9034-2925
FU National Science Foundation [AGS-1159353]
FX The authors acknowledge funding from National Science Foundation grant
AGS-1159353. Valuable comments from the anonymous referee and E. Pariat
are acknowledged. SDO is a mission for NASA's Living With a Star
program. Data are provided courtesy of NASA/SDO and the AIA and HMI
science teams. Hinode is a Japanese mission developed and launched by
ISAS/JAXA, with NAOJ as domestic partner and NASA and STFC (UK) as
international partners. It is operated by these agencies in co-operation
with ESA and NSC (Norway).
NR 31
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U2 5
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0038-0938
EI 1573-093X
J9 SOL PHYS
JI Sol. Phys.
PD SEP
PY 2014
VL 289
IS 9
BP 3313
EP 3329
DI 10.1007/s11207-014-0484-z
PG 17
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AL3AL
UT WOS:000338997200005
ER
PT J
AU Karna, N
Webber, SAH
Pesnell, WD
AF Karna, N.
Webber, S. A. Hess
Pesnell, W. D.
TI Using Polar Coronal Hole Area Measurements to Determine the Solar Polar
Magnetic Field Reversal in Solar Cycle 24
SO SOLAR PHYSICS
LA English
DT Article
DE Coronal holes; Solar cycle; Magnetic reversal; Observation
ID EXTREME-ULTRAVIOLET OBSERVATIONS
AB An analysis of solar polar coronal hole (PCH) areas since the launch of the Solar Dynamics Observatory (SDO) shows how the polar regions have evolved during Solar Cycle 24. We present PCH areas from mid-2010 through 2013 using data from the Atmospheric Imager Assembly (AIA) and Helioseismic and Magnetic Imager (HMI) instruments onboard SDO. Our analysis shows that both the northern and southern PCH areas have decreased significantly in size since 2010. Linear fits to the areas derived from the magnetic-field properties indicate that, although the northern hemisphere went through polar-field reversal and reached solar-maximum conditions in mid-2012, the southern hemisphere had not reached solar-maximum conditions in the polar regions by the end of 2013. Our results show that solar-maximum conditions in each hemisphere, as measured by the area of the polar coronal holes and polar magnetic field, will be offset in time.
C1 [Karna, N.; Webber, S. A. Hess; Pesnell, W. D.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Karna, N.; Webber, S. A. Hess] George Mason Univ, Fairfax, VA 22030 USA.
RP Pesnell, WD (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
EM nkarna@masonlive.gmu.edu; shessweb@masonlive.gmu.edu;
william.d.pesnell@nasa.gov
RI Pesnell, William/D-1062-2012;
OI Pesnell, William/0000-0002-8306-2500; Hess Webber, Shea
A/0000-0002-3631-6491
FU Schlumberger Foundation Faculty for the Future; Catholic University of
America; NASA's Solar Dynamics Observatory
FX N. Karna thanks the Schlumberger Foundation Faculty for the Future for
supporting this research. S. A. Hess Webber thanks the Catholic
University of America and NASA's Solar Dynamics Observatory for
supporting this research. The AIA and HMI data are courtesy of NASA/SDO
and the AIA and HMI Science Investigation Teams. The HMI radial synoptic
maps are available at the Stanford website. The GMU AIA Synoptic Maps
Dataset can be accessed at the George Mason University (GMU) Space
Weather Lab. The EIT images are courtesy of the SOHO/EIT consortium.
SOHO is a mission of international cooperation between ESA and NASA. The
MDI images are provided by the Solar Oscillations Investigation (SOI)
team at the Stanford-Lockheed Institute for Space Research. Daily
sunspot areas dataset were obtained from NASA/Marshall Solar Physics.
Daily values of International Sunspot Number, [RZ], were
obtained from the National Geophysical Data Center in Boulder, CO, USA.
NR 22
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U1 0
U2 4
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0038-0938
EI 1573-093X
J9 SOL PHYS
JI Sol. Phys.
PD SEP
PY 2014
VL 289
IS 9
BP 3381
EP 3390
DI 10.1007/s11207-014-0541-7
PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AL3AL
UT WOS:000338997200009
ER
PT J
AU Duvall, TL
Hanasoge, SM
Chakraborty, S
AF Duvall, T. L., Jr.
Hanasoge, S. M.
Chakraborty, S.
TI Additional Evidence Supporting a Model of Shallow, High-Speed
Supergranulation
SO SOLAR PHYSICS
LA English
DT Article
DE Helioseismology, observations; Helioseismology, direct modeling;
Interior, convective zone; Supergranulation; Velocity fields, interior
ID TIME-DISTANCE HELIOSEISMOLOGY; SOLAR INTERIOR; TRAVEL-TIMES; FLOWS;
INVERSIONS; ATMOSPHERE; KERNELS
AB Recently, Duvall and Hanasoge (Solar Phys. 287, 71, 2013) found that large-distance separation [Delta] travel-time differences from a center to an annulus [delta t (oi)] implied a model of the average supergranular cell that has a peak upflow of 240 m s(-1) at a depth of 2.3 Mm and a corresponding peak outward horizontal flow of 700 m s(-1) at a depth of 1.6 Mm. In the present work, this effect is further studied by measuring and modeling center-to-quadrant travel-time differences [delta t (qu)], which roughly agree with this model. Simulations are analyzed that show that such a model flow would lead to the expected travel-time differences. As a check for possible systematic errors, the center-to-annulus travel-time differences [delta t (oi)] are found not to vary with heliocentric angle. A consistency check finds an increase of delta t (oi) with the temporal frequency [nu] by a factor of two, which is not predicted by the ray theory.
C1 [Duvall, T. L., Jr.] NASA, Goddard Space Flight Ctr, Solar Phys Lab, Greenbelt, MD 20771 USA.
[Hanasoge, S. M.] Tata Inst Fundamental Res, Bombay 400005, Maharashtra, India.
[Hanasoge, S. M.] Max Planck Inst Sonnensyst Forsch, D-37077 Gottingen, Germany.
[Chakraborty, S.] Stanford Univ, WW Hansen Expt Phys Lab, Stanford, CA 94305 USA.
RP Duvall, TL (reprint author), NASA, Goddard Space Flight Ctr, Solar Phys Lab, Greenbelt, MD 20771 USA.
EM Thomas.L.Duvall@nasa.gov; hanasoge@tifr.res.in; deepc@stanford.edu
FU NASA SDO
FX The data used here are courtesy of NASA/SDO and the HMI Science Team. We
thank the HMI team members for their hard work. This work is supported
by NASA SDO.
NR 27
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PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0038-0938
EI 1573-093X
J9 SOL PHYS
JI Sol. Phys.
PD SEP
PY 2014
VL 289
IS 9
BP 3421
EP 3433
DI 10.1007/s11207-014-0537-3
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AL3AL
UT WOS:000338997200012
ER
PT J
AU Nagashima, K
Loptien, B
Gizon, L
Birch, AC
Cameron, R
Couvidat, S
Danilovic, S
Fleck, B
Stein, R
AF Nagashima, Kaori
Loeptien, Bjoern
Gizon, Laurent
Birch, Aaron C.
Cameron, Robert
Couvidat, Sebastien
Danilovic, Sanja
Fleck, Bernhard
Stein, Robert
TI Interpreting the Helioseismic and Magnetic Imager (HMI) Multi-Height
Velocity Measurements
SO SOLAR PHYSICS
LA English
DT Article
DE Velocity fields, photosphere; Oscillations, solar; Helioseismology,
observations
ID SCALE CONVECTION SIMULATIONS; DYNAMICS-OBSERVATORY SDO; SOLAR
PHOTOSPHERE; GRAVITY-WAVES; OSCILLATION MODES; ENERGY FLUX; ATMOSPHERE;
CHROMOSPHERE; SURFACE; MURAM
AB The Solar Dynamics Observatory/Helioseismic and Magnetic Imager (SDO/HMI) filtergrams, taken at six wavelengths around the Fe i 6173.3 line, contain information about the line-of-sight velocity over a range of heights in the solar atmosphere. Multi-height velocity inferences from these observations can be exploited to study wave motions and energy transport in the atmosphere. Using realistic convection-simulation datasets provided by the STAGGER and MURaM codes, we generate synthetic filtergrams and explore several methods for estimating Dopplergrams. We investigate at which height each synthetic Dopplergram correlates most strongly with the vertical velocity in the model atmospheres. On the basis of the investigation, we propose two Dopplergrams other than the standard HMI-algorithm Dopplergram produced from HMI filtergrams: a line-center Dopplergram and an average-wing Dopplergram. These two Dopplergrams correlate most strongly with vertical velocities at the heights of 30 -aEuro parts per thousand 40 km above (line center) and 30 -aEuro parts per thousand 40 km below (average wing) the effective height of the HMI-algorithm Dopplergram. Therefore, we can obtain velocity information from two layers separated by about a half of a scale height in the atmosphere, at best. The phase shifts between these multi-height Dopplergrams from observational data as well as those from the simulated data are also consistent with the height-difference estimates in the frequency range above the photospheric acoustic-cutoff frequency.
C1 [Nagashima, Kaori; Gizon, Laurent; Birch, Aaron C.; Cameron, Robert; Danilovic, Sanja] Max Planck Inst Sonnensyst Forsch, D-37077 Gottingen, Germany.
[Loeptien, Bjoern; Gizon, Laurent] Univ Gottingen, Inst Astrophys, D-37077 Gottingen, Germany.
[Couvidat, Sebastien] Stanford Univ, Stanford, CA 94305 USA.
[Fleck, Bernhard] NASA, Goddard Space Flight Ctr, ESA Sci Operat Dept, Greenbelt, MD 20771 USA.
[Stein, Robert] Michigan State Univ, E Lansing, MI 48824 USA.
RP Nagashima, K (reprint author), Max Planck Inst Sonnensyst Forsch, Justus von Liebig Weg 3, D-37077 Gottingen, Germany.
EM nagashima@mps.mpg.de
OI Nagashima, Kaori/0000-0002-6927-2392
FU IMPRS Solar System School; EU; DFG [SFB 963]; NASA [NNX12AH49G]; NSF
[AGS1141921]; German Aerospace Center (DLR)
FX BL acknowledges support from the IMPRS Solar System School. BL computed
the line profiles from the STAGGER data cubes and the response functions
using the SPINOR code. We thank Michiel van Noort, Thomas Straus, and
Jesper Schou for helpful discussions and comments. KN and LG acknowledge
support from EU FP7 Collaborative Project "Exploitation of Space Data
for Innovative Helio- and Asteroseismology" (SPACEINN). LG acknowledges
support from DFG SFB 963 "Astrophysical Flow Instabilities and
Turbulence" (Project A1). The HMI data used are courtesy of NASA/SDO and
the HMI science team. This work was carried out using the data from the
SDO HMI/AIA Joint Science Operations Center Data Record Management
System and Storage Unit Management System (JSOC DRMS/SUMS). The NSO/Kitt
Peak FTS data used here were produced by NSF/NSO. RS acknowledges
support by NASA grant NNX12AH49G and NSF grant AGS1141921. The STAGGER
calculations were performed on the Pleiades cluster of the NASA Advanced
Supercomputing Division at Ames Research Center. The German Data Center
for SDO (GDC-SDO), funded by the German Aerospace Center (DLR), provided
the IT infrastructure to process the data.
NR 37
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PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0038-0938
EI 1573-093X
J9 SOL PHYS
JI Sol. Phys.
PD SEP
PY 2014
VL 289
IS 9
BP 3457
EP 3481
DI 10.1007/s11207-014-0543-5
PG 25
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AL3AL
UT WOS:000338997200014
ER
PT J
AU Hoeksema, JT
Liu, Y
Hayashi, K
Sun, XD
Schou, J
Couvidat, S
Norton, A
Bobra, M
Centeno, R
Leka, KD
Barnes, G
Turmon, M
AF Hoeksema, J. Todd
Liu, Yang
Hayashi, Keiji
Sun, Xudong
Schou, Jesper
Couvidat, Sebastien
Norton, Aimee
Bobra, Monica
Centeno, Rebecca
Leka, K. D.
Barnes, Graham
Turmon, Michael
TI The Helioseismic and Magnetic Imager (HMI) Vector Magnetic Field
Pipeline: Overview and Performance
SO SOLAR PHYSICS
LA English
DT Article
DE Magnetic fields, photosphere; HMI: vector field; Solar active regions
ID QUIET ACTIVE REGIONS; DYNAMICS-OBSERVATORY SDO; MAJOR SOLAR-FLARES;
MAGNETOGRAMS; AMBIGUITY; MISSION; SAMPLE
AB The Helioseismic and Magnetic Imager (HMI) began near-continuous full-disk solar measurements on 1 May 2010 from the Solar Dynamics Observatory (SDO). An automated processing pipeline keeps pace with observations to produce observable quantities, including the photospheric vector magnetic field, from sequences of filtergrams. The basic vector-field frame list cadence is 135 seconds, but to reduce noise the filtergrams are combined to derive data products every 720 seconds. The primary 720 s observables were released in mid-2010, including Stokes polarization parameters measured at six wavelengths, as well as intensity, Doppler velocity, and the line-of-sight magnetic field. More advanced products, including the full vector magnetic field, are now available. Automatically identified HMI Active Region Patches (HARPs) track the location and shape of magnetic regions throughout their lifetime.
The vector field is computed using the Very Fast Inversion of the Stokes Vector (VFISV) code optimized for the HMI pipeline; the remaining 180(a similar to) azimuth ambiguity is resolved with the Minimum Energy (ME0) code. The Milne-Eddington inversion is performed on all full-disk HMI observations. The disambiguation, until recently run only on HARP regions, is now implemented for the full disk. Vector and scalar quantities in the patches are used to derive active region indices potentially useful for forecasting; the data maps and indices are collected in the SHARP data series, hmi.sharp_720s. Definitive SHARP processing is completed only after the region rotates off the visible disk; quick-look products are produced in near real time. Patches are provided in both CCD and heliographic coordinates.
HMI provides continuous coverage of the vector field, but has modest spatial, spectral, and temporal resolution. Coupled with limitations of the analysis and interpretation techniques, effects of the orbital velocity, and instrument performance, the resulting measurements have a certain dynamic range and sensitivity and are subject to systematic errors and uncertainties that are characterized in this report.
C1 [Hoeksema, J. Todd; Liu, Yang; Hayashi, Keiji; Sun, Xudong; Schou, Jesper; Couvidat, Sebastien; Norton, Aimee; Bobra, Monica] Stanford Univ, WW Hansen Expt Phys Lab, Stanford, CA 94305 USA.
[Centeno, Rebecca] High Altitude Observ NCAR, Boulder, CO USA.
[Leka, K. D.; Barnes, Graham] Northwest Res Associates Inc, Boulder, CO USA.
[Turmon, Michael] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Schou, Jesper] Max Planck Inst Sonnensyst Forsch, D-37077 Gottingen, Germany.
RP Hoeksema, JT (reprint author), Stanford Univ, WW Hansen Expt Phys Lab, Stanford, CA 94305 USA.
EM todd@sun.stanford.edu
RI Sun, Xudong/M-3245-2013
OI Sun, Xudong/0000-0003-4043-616X
FU NASA [NAS5-02139, NNH09CF22C]; National Science Foundation; NASA/Goddard
Space Flight Center [PO#NNG12PP28D/C#GS-23F-0197P]; EU
FX We thank the numerous team members who have contributed to the success
of the SDO mission and particularly to the HMI instrument. This work was
supported by NASA Contract NAS5-02139 (HMI) to Stanford University. Some
of the research described here was carried out by staff of the Jet
Propulsion Laboratory, California Institute of Technology. HAO/NCAR is
supported by the National Science Foundation. Efforts at NWRA were also
supported through NASA Contract NNH09CF22C and by
PO#NNG12PP28D/C#GS-23F-0197P from NASA/Goddard Space Flight Center. J.
Schou acknowledges support from EU FP7 Collaborative Project
Exploitation of Space Data for Innovative Helio- and Asteroseismology
(SPACEINN).
NR 50
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U2 2
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0038-0938
EI 1573-093X
J9 SOL PHYS
JI Sol. Phys.
PD SEP
PY 2014
VL 289
IS 9
BP 3483
EP 3530
DI 10.1007/s11207-014-0516-8
PG 48
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AL3AL
UT WOS:000338997200015
ER
PT J
AU Bobra, MG
Sun, X
Hoeksema, JT
Turmon, M
Liu, Y
Hayashi, K
Barnes, G
Leka, KD
AF Bobra, M. G.
Sun, X.
Hoeksema, J. T.
Turmon, M.
Liu, Y.
Hayashi, K.
Barnes, G.
Leka, K. D.
TI The Helioseismic and Magnetic Imager (HMI) Vector Magnetic Field
Pipeline: SHARPs - Space-Weather HMI Active Region Patches
SO SOLAR PHYSICS
LA English
DT Article
DE Active regions, magnetic fields; Flares, relation to magnetic field;
Instrumentation and data management
ID MAJOR SOLAR-FLARES; NULL POINTS; ENERGY; FLUX; MAGNETOGRAMS; HELICITY;
SHEAR; PRODUCTIVITY; EMERGENCE; EVOLUTION
AB A new data product from the Helioseismic and Magnetic Imager (HMI) onboard the Solar Dynamics Observatory (SDO) called Space-weather HMI Active Region Patches (SHARPs) is now available. SDO/HMI is the first space-based instrument to map the full-disk photospheric vector magnetic field with high cadence and continuity. The SHARP data series provide maps in patches that encompass automatically tracked magnetic concentrations for their entire lifetime; map quantities include the photospheric vector magnetic field and its uncertainty, along with Doppler velocity, continuum intensity, and line-of-sight magnetic field. Furthermore, keywords in the SHARP data series provide several parameters that concisely characterize the magnetic-field distribution and its deviation from a potential-field configuration. These indices may be useful for active-region event forecasting and for identifying regions of interest. The indices are calculated per patch and are available on a twelve-minute cadence. Quick-look data are available within approximately three hours of observation; definitive science products are produced approximately five weeks later. SHARP data are available at jsoc.stanford.edu and maps are available in either of two different coordinate systems. This article describes the SHARP data products and presents examples of SHARP data and parameters.
C1 [Bobra, M. G.; Sun, X.; Hoeksema, J. T.; Liu, Y.; Hayashi, K.] Stanford Univ, WW Hansen Expt Phys Lab, Stanford, CA 94305 USA.
[Turmon, M.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Barnes, G.; Leka, K. D.] Northwest Res Associates Inc, Boulder, CO USA.
RP Hoeksema, JT (reprint author), Stanford Univ, WW Hansen Expt Phys Lab, Stanford, CA 94305 USA.
EM jthoeksema@sun.stanford.edu
RI Sun, Xudong/M-3245-2013
OI Sun, Xudong/0000-0003-4043-616X
FU NASA [NAS5-02139, NNH09CF22C, NNH12CG10C]; NASA/Goddard Space Flight
Center [NNG12PP28D/C# GS-23F-0197P]
FX We thank the many team members who have contributed to the success of
the SDO mission and particularly to the HMI instrument. This work was
supported by NASA Contract NAS5-02139 (HMI) to Stanford University. Some
of the research described here was carried out by staff of the Jet
Propulsion Laboratory, California Institute of Technology. Efforts at
NWRA were also supported through NASA Contracts NNH09CF22C and
NNH12CG10C and by NNG12PP28D/C# GS-23F-0197P from NASA/Goddard Space
Flight Center. The authors thank Huned Botee for development of the
SHARP Data Viewer.
NR 58
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PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0038-0938
EI 1573-093X
J9 SOL PHYS
JI Sol. Phys.
PD SEP
PY 2014
VL 289
IS 9
BP 3549
EP 3578
DI 10.1007/s11207-014-0529-3
PG 30
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AL3AL
UT WOS:000338997200017
ER
PT J
AU Ault, JS
Smith, SG
Browder, JA
Nuttle, W
Franklin, EC
Luo, J
DiNardoe, GT
Bohnsack, JA
AF Ault, J. S.
Smith, S. G.
Browder, J. A.
Nuttle, W.
Franklin, E. C.
Luo, J.
DiNardoe, G. T.
Bohnsack, J. A.
TI Indicators for assessing the ecological dynamics and sustainability of
southern Florida's coral reef and coastal fisheries
SO ECOLOGICAL INDICATORS
LA English
DT Article
DE Average size; Length-based assessment; Fishery exploitation;
Community-level sustainability
ID LENGTH-BASED ASSESSMENT; STOCK PRODUCTION MODEL; FISH STOCKS; REFERENCE
POINTS; AVERAGE-LENGTH; MANAGEMENT; PERFORMANCE; SITUATIONS; MORTALITY;
STEEPNESS
AB Commercial and recreational fisheries target hundreds of fish and shellfish species across the seascape of southern Florida including inshore coastal bays, the flats of barrier islands, coral reefs and offshore pelagic waters. The ecological dynamics and economic sustainability of these valuable fishery resources are key conservation concerns. This study examined two ecological indicators of fishing impacts on exploited populations: (1) the more traditional metric catch per unit of fishing effort (CPUE); and (2) the non-traditional metric average length (L) in the exploited life stage of a population. We show that both indicators were closely related to stock productivity via fisheries population dynamics theory, and that either indicator could be used to estimate fishing mortality rates (F). Data requirements are much less stringent for estimating F from the L indicator than CPUE, making it more practical for data-poor situations common to tropical marine fisheries. Using indicator-based estimates of F within a population dynamic modeling framework enabled an evaluation of fishing impacts on sustainability at both the species and community levels, an important step toward ecosystem-based fisheries assessment and management. A comparison of these approaches applied to the assessment of southern Florida coral reef fisheries suggested that fishing has fundamentally altered the ecological structure of the fish community by depleting the biomass of higher-trophic level carnivores to the extent that the stocks are unsustainable. (C) 2014 Elsevier Ltd. All rights reserved.
C1 [Ault, J. S.; Smith, S. G.; Luo, J.] Univ Miami, Rosenstiel Sch Marine & Atmospher Sci, Miami, FL 33149 USA.
[Browder, J. A.; Bohnsack, J. A.] Natl Marine Fisheries Serv, Southeast Fisheries Sci Ctr, Miami, FL 33149 USA.
[Nuttle, W.] Ecohydrol Com, Ottawa, ON K1SB46, Canada.
[Franklin, E. C.] Univ Hawaii Manoa, Sch Ocean & Earth Sci & Technol, Kaneohe, HI 96744 USA.
[DiNardoe, G. T.] Natl Marine Fisheries Serv, Pacific Isl Fisheries Sci Ctr, Honolulu, HI 96822 USA.
RP Ault, JS (reprint author), Univ Miami, Rosenstiel Sch Marine & Atmospher Sci, 4600 Rickenbacker Causeway, Miami, FL 33149 USA.
EM jault@rsmas.miami.edu
RI Ault, Jerald/A-5241-2008
OI Ault, Jerald/0000-0001-9657-8007
FU NOAA NOS CSCOR Program Award [NA08OAR4320889]; Bonefish and Tarpon
Trust; Robertson Foundation; NOAA Pacific Islands Fisheries Science
Center iREEF (Integrated Reef Ecosystem Evaluation Framework) [WE-
133F-12-SE-2099]; NOAA Pulley Ridge Grant [NA11NOS4780045];
Papahanumokuakea MNS Grant [RA133C12SE2107]; National Fish and Wildlife
Foundation Grant [0302-12-031178]; NOAA Fisheries Coral Reef
Conservation Program Grant [NA17RJ1226]; NOM MARFIN Grant
[NA11NMF4330129]; National Science Foundation [EAR-1204752]
FX We appreciate the technical assistance provided by M.S. Adams, D.R.
Bryan, M.O. Nadon and N.R. Vaughan. This paper is a result of research
under the Marine and Estuarine Goal Setting (MARES) for South Florida
Project funded by NOAA NOS CSCOR Program Award No. NA08OAR4320889,
Bonefish and Tarpon Trust, Robertson Foundation, NOAA Pacific Islands
Fisheries Science Center iREEF (Integrated Reef Ecosystem Evaluation
Framework) Contract No. WE- 133F-12-SE-2099, NOAA Pulley Ridge Grant No.
NA11NOS4780045, Papahanumokuakea MNS Grant No. RA133C12SE2107, National
Fish and Wildlife Foundation Grant No. 0302-12-031178, NOAA Fisheries
Coral Reef Conservation Program Grant No. NA17RJ1226, and the NOM MARFIN
Grant No. NA11NMF4330129. This material was also based upon work
supported by the National Science Foundation under Grant No.
EAR-1204752. This manuscript was greatly improved by the comments of two
anonymous reviewers.
NR 35
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U1 3
U2 58
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 1470-160X
EI 1872-7034
J9 ECOL INDIC
JI Ecol. Indic.
PD SEP
PY 2014
VL 44
SI SI
BP 164
EP 172
DI 10.1016/j.ecolind.2014.04.013
PG 9
WC Biodiversity Conservation; Environmental Sciences
SC Biodiversity & Conservation; Environmental Sciences & Ecology
GA AK7KX
UT WOS:000338608300016
ER
PT J
AU Martin, W
Cairns, B
Bal, G
AF Martin, William
Cairns, Brian
Bal, Guillaume
TI Adjoint methods for adjusting three-dimensional atmosphere and surface
properties to fit multi-angle/multi-pixel polarimetric measurements
SO JOURNAL OF QUANTITATIVE SPECTROSCOPY & RADIATIVE TRANSFER
LA English
DT Article
DE Adjoint methods; Three-dimensional vector radiative transfer;
Linearization; Remote sensing; Parameter derivatives
ID RADIATIVE-TRANSFER MODEL; DISCRETE ORDINATE METHOD; PERTURBATION-THEORY;
SPHERICAL ATMOSPHERE; WEIGHTING FUNCTIONS; OPTICAL TOMOGRAPHY;
FREQUENCY-DOMAIN; RETRIEVAL; VALIDATION; ALGORITHM
AB This paper derives an efficient procedure for using the three-dimensional (3D) vector radiative transfer equation (VRTE) to adjust atmosphere and surface properties and improve their with multi-angle/multi-pixel radiometric and polarimetric measurements of scattered sunlight The proposed adjoint method uses the 3D VRTE to compute the measurement misfit function and the adjoint 3D VRTE to compute its gradient with respect to all unknown parameters. In the remote sensing problems of interest, the scalar-valued misfit function quantifies with data as a function of atmosphere and surface properties, and its gradient guides the search through this parameter space. Remote sensing of the atmosphere and surface in a three-dimensional region may require thousands of unknown parameters and millions of data points. Many approaches would require calls to the 3D VRTE solver in proportion to the number unknown parameters or measurements. To avoid this issue of scale, we focus on computing the gradient of the misfit function as an alternative to the Jacobian of the measurement operator. The resulting adjoint method provides a way to adjust 3D atmosphere and surface properties with only two calls to the 3D VRTE solver for each spectral channel, regardless of the number retrieval parameters, measurement view angles or pixels. This gives a procedure for adjusting atmosphere and surface parameters that will scale to the large problems of 3D remote sensing. For certain types of multi-angle/multi-pixel polarimetric measurements, this encourages the development of a new class of three-dimensional retrieval algorithms with more flexible parametrizations of spatial heterogeneity, less reliance on data screening procedures, and improved coverage in terms of the resolved physical processes in the Earth's atmosphere. (C) 2014 Elsevier Ltd. All rights reserved.
C1 [Martin, William; Bal, Guillaume] Columbia Univ, Dept Appl Phys & Appl Math, New York, NY 10027 USA.
[Cairns, Brian] NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
RP Martin, W (reprint author), Columbia Univ, Dept Appl Phys & Appl Math, New York, NY 10027 USA.
EM wgm2111@columbia.edu
OI Cairns, Brian/0000-0002-1980-1022
FU NASA Head-quarters under the NASA Earth and Space Science Fellowship
Program [NNX-10AN85H]; US National Science Foundation to Columbia
University; Aerosol Cloud Ecosystem (ACE) mission by NASA Head-quarters;
ACE program scientists Hal Mating and Paula Bontempi; NASA/ESTO's AIST
program [1497551]; NSF [DMS-1108608]
FX William Martin acknowledges support from NASA Head-quarters under the
NASA Earth and Space Science Fellowship Program, Grant NNX-10AN85H, and
he was partially funded by an IGERT grant from the US National Science
Foundation to Columbia University Also, he is grateful to Alexander
Kokhanovsky for organizing a workshop on aerosol remote sensing from
space (July 15-19, 2013; International Space Sciences Institute, Bern,
CH) and to Thomas Trautmann, Anthony Davis, and the other participants
for encouragement and fruitful discussions. Brian Cairns would like to
acknowledge support of the work presented here under pre-formulation
funding of the Aerosol Cloud Ecosystem (ACE) mission by NASA
Head-quarters and the ACE program scientists Hal Mating and Paula
Bontempi. Guillaume Bal acknowledges support, through JPL Subcontract
no. 1497551, from NASA/ESTO's AIST program (3D-TRACE project), and from
the NSF under Grant DMS-1108608.
NR 45
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U1 0
U2 10
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0022-4073
EI 1879-1352
J9 J QUANT SPECTROSC RA
JI J. Quant. Spectrosc. Radiat. Transf.
PD SEP
PY 2014
VL 144
BP 68
EP 85
DI 10.1016/j.jqsrt.2014.03.030
PG 18
WC Optics; Spectroscopy
SC Optics; Spectroscopy
GA AJ9AS
UT WOS:000337999800006
ER
PT J
AU Majurec, N
Johnson, JT
Tanelli, S
Durden, SL
AF Majurec, Ninoslav
Johnson, Joel T.
Tanelli, Simone
Durden, Stephen L.
TI Comparison of Model Predictions With Measurements of Ku- and Ka-Band
Near-Nadir Normalized Radar Cross Sections of the Sea Surface From the
Genesis and Rapid Intensification Processes Experiment
SO IEEE TRANSACTIONS ON GEOSCIENCE AND REMOTE SENSING
LA English
DT Article
DE Airborne radar; doppler radar; meteorological radar; radar
cross-sections; radar remote sensing; sea surface
ID TRMM PRECIPITATION RADAR; SLOPE; WAVES; BACKSCATTER; SCATTERING;
ALTIMETER; ROUGHNESS; SIGNALS
AB A comparison of model predictions with measurements of near-nadir normalized radar cross sections (NRCSs) of the sea surface at Ku- and Ka-bands is reported. Measurements of Airborne Precipitation Radar Second Generation (APR-2) from near nadir to 25 degrees incidence angle, along with simultaneous wind truth from dropsonde observations, are compared with predictions of the "cutoff-invariant" two-scale model of sea scattering with the overall goal of assessing the model for possible future use in the APR-2 calibration process. The performance of the model as a function of wind speed and incidence angle is therefore emphasized. The measured data set, acquired primarily during the 2010 "Genesis and Rapid Intensification Processes" (GRIP) experiment, includes wind speeds from approximately 5 to 45 m/s. Model comparisons are limited by uncertainties in the wind fields due to limited dropsonde coverage; the data set is separated into "more reliable" (containing wind speeds of 5-20 m/s) and "less reliable" (wind speeds of 5-45 m/s) wind truth categories accordingly. Because a model of the sea spectrum is required for cutoff-invariant model predictions, comparisons with measured data are performed for three differing sea spectrum descriptions. It is found that a bias of less than similar to 1 dB over the wind speed range 5-40 m/s and a standard deviation less than 1 dB over the wind speed range 10-40 m/s can be achieved when using the "unified" sea spectrum description of Elfouhaily et al. The model also provides error levels that are near uniform with respect to both incidence angle and wind speed.
C1 [Majurec, Ninoslav] Ohio State Univ, Dept Elect Engn & Comp, ElectroSci Lab, Columbus, OH 43212 USA.
[Johnson, Joel T.] Ohio State Univ, Dept Elect & Comp Engn, ElectroSci Lab, Columbus, OH 43212 USA.
[Tanelli, Simone; Durden, Stephen L.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Majurec, N (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
FU NASA Precipitation Measurement Missions Program; National Aeronautics
and Space Administration
FX This work was performed in support to NASA Precipitation Measurement
Missions Program, and it was made possible by the data acquired during
the Genesis and Rapid Intensification Processes (GRIP) project. A
portion of this work (S. L. Durden and S. Tanelli) 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 25
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U1 1
U2 16
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 SEP
PY 2014
VL 52
IS 9
BP 5320
EP 5332
DI 10.1109/TGRS.2013.2288105
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 AI8MU
UT WOS:000337171900005
ER
PT J
AU Paillou, P
Sufyar, S
Freeman, A
AF Paillou, Philippe
Sufyar, Sarah
Freeman, Anthony
TI The Chott El Djerid, Tunisia: Observation and Discussion of a SAR Phase
Signature Over Evaporitic Soils
SO IEEE TRANSACTIONS ON GEOSCIENCE AND REMOTE SENSING
LA English
DT Article
DE Chott; El Djerid; integral equation model (IEM); phase; playa;
polarimetry; synthetic aperture radar (SAR); Tunisia
ID WET SUBSURFACE STRUCTURES; POLARIMETRIC L-BAND; SOUTHERN TUNISIA;
DIELECTRIC-PROPERTIES; PLAYA; BACKSCATTERING; AVHRR
AB The presence of water in arid regions is correlated to large evaporitic deposits, with high concentration of salts. Polarimetric synthetic aperture radar (SAR) observations over such areas show high variations for both the amplitude and phase of the backscattered copolarized signal. This is due to a large dynamic range for both surface roughness and dielectric constant parameters, between the wet and dry seasons: crystallized salt is rough and presents a low dielectric constant, whereas saline water corresponds to smooth and conductive surfaces. We observed a complete seasonal cycle over the chott El Djerid playa, in southern Tunisia, using the 5.6-GHz C-band polarimetric SAR on-board RADARSAT-2. One SAR image acquisition was performed every 24 days, from February to September 2009. In addition to expected variations in the radar backscattered power, we observed significant changes in the phase difference between horizontally and vertically polarized channels. In order to explain such a phase effect, we first considered the arguments of the Fresnel reflectivity coefficient when approaching the Brewster angle, for materials presenting a high loss tangent. A more complete analytical modeling derived from the integral equation model approach confirmed this hypothesis.
C1 [Paillou, Philippe; Sufyar, Sarah] Univ Bordeaux, UMR 5804, LAB, F-33270 Floirac, France.
[Sufyar, Sarah] Lab Integrat Mat Syst IMS, F-33607 Pessac, France.
[Freeman, Anthony] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Paillou, P (reprint author), Univ Bordeaux, UMR 5804, LAB, F-33270 Floirac, France.
EM paillou@obs.u-bordeaux1.fr
FU French Space Agency (CNES); Programme National de Teledetection Spatiale
(INSU)
FX This work was supported in part by the French Space Agency (CNES) and in
part by the Programme National de Teledetection Spatiale (INSU).
NR 26
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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
EI 1558-0644
J9 IEEE T GEOSCI REMOTE
JI IEEE Trans. Geosci. Remote Sensing
PD SEP
PY 2014
VL 52
IS 9
BP 5798
EP 5806
DI 10.1109/TGRS.2013.2292822
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 AI8MU
UT WOS:000337171900047
ER
PT J
AU Jimenez-Munoz, JC
Sobrino, JA
Mattar, C
Hulley, G
Gottsche, FM
AF Jimenez-Munoz, Juan C.
Sobrino, Jose A.
Mattar, Cristian
Hulley, Glynn
Goettsche, Frank-M.
TI Temperature and Emissivity Separation From MSG/SEVIRI Data
SO IEEE TRANSACTIONS ON GEOSCIENCE AND REMOTE SENSING
LA English
DT Article
DE MODIS; SEVIRI; surface emissivity; surface temperature; TES
ID LAND-SURFACE TEMPERATURE; ASTER TEMPERATURE; ALGORITHM; PRODUCTS;
VALIDATION; RETRIEVAL; SEA
AB In this paper, we analyze the feasibility of applying the temperature and emissivity separation (TES) algorithm to thermal-infrared data acquired with three bands of the Spinning Enhanced Visible and Infrared Imager (SEVIRI) onboard the Meteosat Second Generation platform (SEVTES). The performance of the SEVTES algorithm was tested using data simulated over different atmospheric conditions and surface emissivities, with errors around 1.5% for emissivity and 1.5 K for temperature when atmospheric correction is accurate enough. In contrast, errors on land-leaving radiances higher than 2% or uncertainties on total atmospheric water vapor amount higher than 5% lead to errors on emissivity higher than 2% and errors on land surface temperature higher than 3 K, especially when the atmospheric absorption is overestimated. SEVIRI data acquired in August 2011 were also used to validate SEVTES emissivities against in situ measurements collected in five different homogeneous areas over Africa. Values were also intercompared to Moderate Resolution Imaging Spectroradiometer (MODIS)-derived and Advanced Spaceborne Thermal Emission and Reflection Radiometer (ASTER)-derived emissivities and to the LSA SAF emissivity product. Results show that SEVTES-derived emissivity values are consistent with MODIS-TES and ASTER-TES retrievals and that SEVTES also improves the retrievals included in LSA SAF and MOD11Cx v5 products. When compared to laboratory measurements, accuracies of around 1%-2% were obtained, although occasional inaccuracies (2%-3%) were also found in some cases at band 8.7 mu m. The results presented in this paper show the potential SEVTES has for improving the LSA SAF product over arid and semiarid areas.
C1 [Jimenez-Munoz, Juan C.; Sobrino, Jose A.] Univ Valencia, Image Proc Lab, Global Change Unit, Valencia 46071, Spain.
[Mattar, Cristian] Univ Santiago, Dept Environm Sci & Renewable Nat Resources, Lab Anal Biosphere, Santiago 11315, Chile.
[Hulley, Glynn] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Goettsche, Frank-M.] Karlsruhe Inst Technol, D-76344 Eggenstein Leopoldshafen, Germany.
RP Jimenez-Munoz, JC (reprint author), Univ Valencia, Image Proc Lab, Global Change Unit, Valencia 46071, Spain.
EM jcjm@uv.es; sobrino@uv.es; cristian.mattar@uv.es;
glynn.hulley@jpl.nasa.gov; frank.goettsche@kit.edu
RI Sobrino, Jose/M-1585-2014; Mattar, Cristian/P-6711-2014; Gottsche,
Frank-Michael/A-7362-2013; Jimenez-Munoz, Juan Carlos/K-2903-2015
OI Sobrino, Jose/0000-0003-3787-9373; Gottsche,
Frank-Michael/0000-0001-5836-5430; Jimenez-Munoz, Juan
Carlos/0000-0001-7562-4895
FU European Union (CEOP-AEGIS) [212921]; Ministerio de Economia y
Competitividad (EODIX) [AYA2008-0595-C04-01]; Ministerio de Economia y
Competitividad (CEOS-Spain) [AYA2011-29334-C02-01]; Universitat de
Valencia [UV-INV-PRECOMP13-115366]
FX This work was supported by the European Union (CEOP-AEGIS, project
FP7-ENV-2007-1 Proposal No. 212921), the Ministerio de Economia y
Competitividad (EODIX, project AYA2008-0595-C04-01; CEOS-Spain, project
AYA2011-29334-C02-01), and the Universitat de Valencia
(UV-INV-PRECOMP13-115366).
NR 37
TC 11
Z9 11
U1 0
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 SEP
PY 2014
VL 52
IS 9
BP 5937
EP 5951
DI 10.1109/TGRS.2013.2293791
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 AI8MU
UT WOS:000337171900058
ER
PT J
AU Ouellette, JD
Johnson, JT
Kim, S
van Zyl, JJ
Moghaddam, M
Spencer, MW
Tsang, L
Entekhabi, D
AF Ouellette, Jeffrey D.
Johnson, Joel T.
Kim, Seungbum
van Zyl, Jakob J.
Moghaddam, Mahta
Spencer, Michael W.
Tsang, Leung
Entekhabi, Dara
TI A Simulation Study of Compact Polarimetry for Radar Retrieval of Soil
Moisture
SO IEEE TRANSACTIONS ON GEOSCIENCE AND REMOTE SENSING
LA English
DT Article
DE Compact polarimetry; data cube; retrieval algorithm; soil moisture; time
series
AB A compact polarimetric (CP) radar system requires fewer measurements than a fully polarimetric (FP) system, thus allowing added flexibility in radar system design. Previous studies have shown the potential of using compact polarimetry for radar remote sensing of soil moisture. This paper extends previous studies by considering a time series data cube retrieval algorithm and measurements in the presence of vegetation. Vegetation information is assumed to be provided by an ancillary data source in the retrieval process. The performance of an algorithm for reconstructing FP information from CP measurements of vegetated soil surfaces is also examined. The results of the study show that only a modest degradation in soil moisture retrieval performance occurs when compact-pol measurements are used in place of full-pol data.
C1 [Ouellette, Jeffrey D.; Johnson, Joel T.] Ohio State Univ, Columbus, OH 43210 USA.
[Kim, Seungbum; van Zyl, Jakob J.; Spencer, Michael W.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Moghaddam, Mahta] Univ So Calif, Los Angeles, CA 90089 USA.
[Tsang, Leung] Univ Washington, Seattle, WA 98195 USA.
[Entekhabi, Dara] MIT, Cambridge, MA 02139 USA.
RP Ouellette, JD (reprint author), Ohio State Univ, Columbus, OH 43210 USA.
EM ouellette.18@osu.edu; johnson@ece.osu.edu
NR 15
TC 3
Z9 4
U1 1
U2 18
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 SEP
PY 2014
VL 52
IS 9
BP 5966
EP 5973
DI 10.1109/TGRS.2013.2294133
PG 8
WC Geochemistry & Geophysics; Engineering, Electrical & Electronic; Remote
Sensing; Imaging Science & Photographic Technology
SC Geochemistry & Geophysics; Engineering; Remote Sensing; Imaging Science
& Photographic Technology
GA AI8MU
UT WOS:000337171900060
ER
PT J
AU Stephens, E
Schumann, G
Bates, P
AF Stephens, Elisabeth
Schumann, Guy
Bates, Paul
TI Problems with binary pattern measures for flood model evaluation
SO HYDROLOGICAL PROCESSES
LA English
DT Article
DE remote sensing; flood modelling; performance measures; calibration;
evaluation
ID FINITE-VOLUME MODEL; RASTER-BASED MODEL; INUNDATION MODELS; CALIBRATION;
UNCERTAINTY; RESOLUTION; EXTENT
AB As the calibration and evaluation of flood inundation models are a prerequisite for their successful application, there is a clear need to ensure that the performance measures that quantify how well models match the available observations are fit for purpose. This paper evaluates the binary pattern performance measures that are frequently used to compare flood inundation models with observations of flood extent. This evaluation considers whether these measures are able to calibrate and evaluate model predictions in a credible and consistent way, i.e. identifying the underlying model behaviour for a number of different purposes such as comparing models of floods of different magnitudes or on different catchments.
Through theoretical examples, it is shown that the binary pattern measures are not consistent for floods of different sizes, such that for the same vertical error in water level, a model of a flood of large magnitude appears to perform better than a model of a smaller magnitude flood. Further, the commonly used Critical Success Index (usually referred to as F-< 2 >) is biased in favour of overprediction of the flood extent, and is also biased towards correctly predicting areas of the domain with smaller topographic gradients. Consequently, it is recommended that future studies consider carefully the implications of reporting conclusions using these performance measures. Additionally, future research should consider whether a more robust and consistent analysis could be achieved by using elevation comparison methods instead. Copyright (C) 2013 John Wiley & Sons, Ltd.
C1 [Stephens, Elisabeth; Schumann, Guy; Bates, Paul] Univ Bristol, Sch Geog Sci, Bristol BS8 1SS, Avon, England.
[Stephens, Elisabeth] Univ Oxford, Dept Phys, Oxford OX1 3PU, England.
[Schumann, Guy] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Stephens, E (reprint author), Univ Bristol, Sch Geog Sci, Univ Rd, Bristol BS8 1SS, Avon, England.
EM stephens@atm.ox.ac.uk
RI Bates, Paul/C-8026-2012; Schumann, Guy/F-9760-2011;
OI Bates, Paul/0000-0001-9192-9963; Stephens, Elisabeth/0000-0002-5439-7563
FU European Union 'KULTURISK' project [FP7-ENV-2010-265280]; joint Great
Western Research and Environment Agency studentship
FX This work is supported by the European Union 'KULTURISK' project via
grant FP7-ENV-2010-265280, and Elisabeth Stephens' time was also funded
by a joint Great Western Research and Environment Agency studentship.
NR 26
TC 8
Z9 8
U1 2
U2 11
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 0885-6087
EI 1099-1085
J9 HYDROL PROCESS
JI Hydrol. Process.
PD AUG 30
PY 2014
VL 28
IS 18
BP 4928
EP 4937
DI 10.1002/hyp.9979
PG 10
WC Water Resources
SC Water Resources
GA AN8YV
UT WOS:000340893000008
ER
PT J
AU Kim, K
Rim, T
Park, C
Kim, D
Meyyappan, M
Lee, JS
AF Kim, Kihyun
Rim, Taiuk
Park, Chanoh
Kim, Donghoon
Meyyappan, M.
Lee, Jeong-Soo
TI Suspended honeycomb nanowire ISFETs for improved stiction-free
performance
SO NANOTECHNOLOGY
LA English
DT Article
DE ion-sensitive field effect transistor; gate-all-around (GAA); honeycomb
structure; stiction; pH sensing; top-down; suspended nanowire
ID FIELD-EFFECT TRANSISTOR; BIOSENSORS; DNA; NANOSENSORS; ADSORPTION;
ELECTRODE; DEVICES; SENSORS; PH
AB This paper reports high performance ion-sensitive field-effect transistors (ISFETs) with a suspended honeycomb nanowire (SHNW) structure. The SHNW can provide a longer, stiction-free channel than that which is possible with a suspended straight nanowire (SSNW) for the realization of gate-all-around biosensors. Devices with SHNWs, SSNWs and conventional nanowires on the substrate have been fabricated using a top-down approach in order to compare their electrical performances. The SHNW devices exhibit excellent electrical characteristics such as lower subthreshold swing, higher transconductance and higher linear drain current. In addition, the SHNW ISFETs show better pH sensitivity than other ISFETs. Based on the results, the SHNW device appears promising for enhancing the intrinsic performance and ensuring the reliable operation of biosensor applications.
C1 [Kim, Kihyun; Kim, Donghoon; Lee, Jeong-Soo] Pohang Univ Sci & Technol POSTECH, Dept Elect Engn, Pohang, South Korea.
[Rim, Taiuk; Meyyappan, M.] Pohang Univ Sci & Technol POSTECH, Dept Creat IT Engn, Pohang, South Korea.
[Rim, Taiuk; Meyyappan, M.] Pohang Univ Sci & Technol POSTECH, Future IT Innovat Lab, Pohang, South Korea.
[Park, Chanoh; Lee, Jeong-Soo] Pohang Univ Sci & Technol POSTECH, Div IT Convergence Engn, Pohang, South Korea.
[Meyyappan, M.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
RP Kim, K (reprint author), Pohang Univ Sci & Technol POSTECH, Dept Elect Engn, Pohang, South Korea.
EM ljs6951@postech.ac.kr
FU National Research Foundation (NRF) [2013R1A1A2007094]; center for
advanced soft electronics under the global frontier research program of
the Ministry of Education, Science, and Technology (MEST)
[2011-0031638]; 'IT Consilience Creative Program'
[NIPA-2014-H0201-14-1001]
FX This work was in part supported by the National Research Foundation
(NRF) (No. 2013R1A1A2007094), by a grant (Code No. 2011-0031638) from
the center for advanced soft electronics under the global frontier
research program of the Ministry of Education, Science, and Technology
(MEST) and by the 'IT Consilience Creative Program'
(NIPA-2014-H0201-14-1001) supervised by the National IT Industry
Promotion Agency, Korea.
NR 32
TC 6
Z9 6
U1 2
U2 20
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0957-4484
EI 1361-6528
J9 NANOTECHNOLOGY
JI Nanotechnology
PD AUG 29
PY 2014
VL 25
IS 34
AR 345501
DI 10.1088/0957-4484/25/34/345501
PG 7
WC Nanoscience & Nanotechnology; Materials Science, Multidisciplinary;
Physics, Applied
SC Science & Technology - Other Topics; Materials Science; Physics
GA AP1DR
UT WOS:000341807100013
PM 25091979
ER
PT J
AU Gershman, DJ
Slavin, JA
Raines, JM
Zurbuchen, TH
Anderson, BJ
Korth, H
Baker, DN
Solomon, SC
AF Gershman, Daniel J.
Slavin, James A.
Raines, Jim M.
Zurbuchen, Thomas H.
Anderson, Brian J.
Korth, Haje
Baker, Daniel N.
Solomon, Sean C.
TI Ion kinetic properties in Mercury's pre-midnight plasma sheet
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
DE mercury; plasma sheet; planetary ion
ID MESSENGER OBSERVATIONS; PLANETARY IONS; MAGNETOSPHERE; MAGNETOMETER;
DYNAMICS; MODEL; MAGNETOPAUSE; ENVIRONMENT; INSTRUMENT
AB With data from the Fast Imaging Plasma Spectrometer sensor on the MErcury Surface, Space ENvironment, GEochemistry, and Ranging spacecraft, we demonstrate that the average distributions for both solar wind and planetary ions in Mercury's pre-midnight plasma sheet are well-described by hot Maxwell-Boltzmann distributions. Temperatures and densities of the H+-dominated plasma sheet, in the ranges similar to 1-10cm(-3) and similar to 5-30MK, respectively, maintain thermal pressures of similar to 1nPa. The dominant planetary ion, Na+, has number densities about 10% that of H+. Solar wind ions retain near-solar-wind abundances with respect to H+ and exhibit mass-proportional ion temperatures, indicative of a reconnection-dominated heating in the magnetosphere. Conversely, planetary ion species are accelerated to similar average energies greater by a factor of similar to 1.5 than that of H+. This energization is suggestive of acceleration in an electric potential, consistent with the presence of a strong centrifugal acceleration process in Mercury's magnetosphere.
C1 [Gershman, Daniel J.] NASA, Goddard Space Flight Ctr, Geospace Phys Lab, Greenbelt, MD 20771 USA.
[Gershman, Daniel J.; Slavin, James A.; Raines, Jim M.; Zurbuchen, Thomas H.] Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA.
[Anderson, Brian J.; Korth, Haje] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD USA.
[Baker, Daniel N.] Univ Colorado, Lab Atmospher & Space Phys, 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 Gershman, DJ (reprint author), NASA, Goddard Space Flight Ctr, Geospace Phys Lab, Greenbelt, MD 20771 USA.
EM djgersh@umich.edu
RI Slavin, James/H-3170-2012
OI Slavin, James/0000-0002-9206-724X
FU NASA Discovery Program [NAS5-97271, NASW-00002]; Goddard Space Flight
Center by NASA Postdoctoral Program
FX 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. DJG
is supported at Goddard Space Flight Center by an appointment to the
NASA Postdoctoral Program administered by Oak Ridge Associated
Universities. Data used in this study are available from the Planetary
Data System.
NR 31
TC 14
Z9 14
U1 0
U2 6
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 AUG 28
PY 2014
VL 41
IS 16
BP 5740
EP 5747
DI 10.1002/2014GL060468
PG 8
WC Geosciences, Multidisciplinary
SC Geology
GA AQ4HT
UT WOS:000342755400007
ER
PT J
AU Besserer, J
Nimmo, F
Wieczorek, MA
Weber, RC
Kiefer, WS
McGovern, PJ
Andrews-Hanna, JC
Smith, DE
Zuber, MT
AF Besserer, Jonathan
Nimmo, Francis
Wieczorek, Mark A.
Weber, Renee C.
Kiefer, Walter S.
McGovern, Patrick J.
Andrews-Hanna, Jeffrey C.
Smith, David E.
Zuber, Maria T.
TI GRAIL gravity constraints on the vertical and lateral density structure
of the lunar crust
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
DE Moon; Lunar crust; Density; Porosity; Admittance; Gravity
ID SPECTRAL ESTIMATION; INTERNAL STRUCTURE; BASIN IMPACT; HEAT-FLOW; MOON;
MISSION; SPHERE; INTERIOR; MEGAREGOLITH; ORBITER
AB We analyzed data from the Gravity Recovery and Interior Laboratory (GRAIL) mission using a localized admittance approach to map out spatial variations in the vertical density structure of the lunar crust. Mare regions are characterized by a distinct decrease in density with depth, while the farside is characterized by an increase in density with depth at an average gradient of approximate to 35kgm(-3)km(-1) and typical surface porosities of at least 20%. The Apollo 12 and 14 landing site region has a similar density structure to the farside, permitting a comparison with seismic velocity profiles. The interior of the South Pole-Aitken (SP-A) impact basin appears distinct with a near-surface low-density (porous) layer 2-3 times thinner than the rest of the farside. This result suggests that redistribution of material during the large SP-A impact likely played a major role in sculpting the lunar crust.
C1 [Besserer, Jonathan; Nimmo, Francis] Univ Calif Santa Cruz, Dept Earth & Planetary Sci, Santa Cruz, CA 95064 USA.
[Wieczorek, Mark A.] Univ Paris Diderot, Inst Phys Globe Paris, Sorbonne Paris Cite, Paris, France.
[Weber, Renee C.] NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA.
[Kiefer, Walter S.; McGovern, Patrick J.] Lunar & Planetary Inst, Ctr Lunar Sci & Explorat, Houston, TX 77058 USA.
[Andrews-Hanna, Jeffrey C.] Colorado Sch Mines, Dept Geophys, Golden, CO 80401 USA.
[Andrews-Hanna, Jeffrey C.] Colorado Sch Mines, Ctr Space Resources, Golden, CO 80401 USA.
[Smith, David E.; Zuber, Maria T.] MIT, Dept Earth Atmospher & Planetary Sci, Cambridge, MA USA.
RP Besserer, J (reprint author), Univ Calif Santa Cruz, Dept Earth & Planetary Sci, Santa Cruz, CA 95064 USA.
EM jbessere@ucsc.edu
RI Wieczorek, Mark/G-6427-2010;
OI Wieczorek, Mark/0000-0001-7007-4222; McGovern,
Patrick/0000-0001-9647-3096; Kiefer, Walter/0000-0001-6741-5460
FU NASA; NASA GRAIL Guest Scientist Program [NNX12AL08G]
FX The GRAIL mission is supported by NASA's Discovery Program and is
performed under contract to the Massachusetts Institute of Technology
and the Jet Propulsion Laboratory, California Institute of Technology.
We are grateful to the Editor, A. J. Dombard, and two anonymous
reviewers for their great help in improving the initial version of the
manuscript. J. B. and F.N. thank the NASA GRAIL Guest Scientist Program
(grant NNX12AL08G), S. G. Mogilevskaya, B. Noyelles, S. Kamata, and T.
Lay for fruitful discussions, and also J. M. Soderblom for comments on
an earlier version of the manuscript. Data used to generate the results
of this paper are available at http://pds-geosciences.wustl.edu and
www.Ipgp.Fr/%7Ewieczor (see also Table S1).
NR 50
TC 18
Z9 18
U1 1
U2 23
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 AUG 28
PY 2014
VL 41
IS 16
BP 5771
EP 5777
DI 10.1002/2014GL060240
PG 7
WC Geosciences, Multidisciplinary
SC Geology
GA AQ4HT
UT WOS:000342755400011
ER
PT J
AU Kliore, AJ
Nagy, A
Asmar, S
Anabtawi, A
Barbinis, E
Fleischman, D
Kahan, D
Klose, J
AF Kliore, Arvydas J.
Nagy, Andrew
Asmar, Sami
Anabtawi, Aseel
Barbinis, Elias
Fleischman, Don
Kahan, Danny
Klose, John
TI The ionosphere of Saturn as observed by the Cassini Radio Science System
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
DE Saturn; ionosphere; Cassini; Radio Science
ID ELECTRON-DENSITY; MODEL; OCCULTATION; ATMOSPHERE
AB Fifty-nine ionsopheric radio occultation observations of the vertical electron density profile in the Saturn ionosphere have been made since the Cassini spacecraft was inserted in orbit around Saturn in 2004. Significant orbit to orbit variations were observed, but the general trend noted in earlier orbits, namely, increasing electron densities with increasing latitude was reconfirmed and bolstered with this extended data base. This trend is likely to be due to some combination of increasing ionization rates and decreasing water influx with latitude.
C1 [Kliore, Arvydas J.; Asmar, Sami; Anabtawi, Aseel; Barbinis, Elias; Fleischman, Don; Kahan, Danny; Klose, John] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
[Nagy, Andrew] Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA.
RP Kliore, AJ (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
EM kliore@juno.com
FU NASA; Cassini project
FX This work was performed at the Jet Propulsion Laboratory, California
Institute of Technology, and the Department of Atmospheric, Oceanic, and
Space Sciences, University of Michigan, under contracts from NASA. The
authors thank the Cassini project for supporting the work presented in
this paper. We also want to thank G. Bjoraker for providing us with yet
unpublished information on water column contents derived from the
Cassini CIRS observations.
NR 13
TC 2
Z9 2
U1 0
U2 4
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 AUG 28
PY 2014
VL 41
IS 16
BP 5778
EP 5782
DI 10.1002/2014GL060512
PG 5
WC Geosciences, Multidisciplinary
SC Geology
GA AQ4HT
UT WOS:000342755400012
ER
PT J
AU Han, SC
Sauber, J
Pollitz, F
AF Han, Shin-Chan
Sauber, Jeanne
Pollitz, Fred
TI Broadscale postseismic gravity change following the 2011 Tohoku-Oki
earthquake and implication for deformation by viscoelastic relaxation
and afterslip
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
DE postseismic gravity; viscoelastic relaxation; afterslip; GRACE; GPS
ID SUMATRA-ANDAMAN EARTHQUAKE; LAYERED SPHERICAL EARTH; CRUSTAL
DEFORMATION; SURFACE-WAVES; GRACE; SLIP; INVERSION; MODEL; ZONES
AB The analysis of GRACE gravity data revealed postseismic gravity increase by 6 Gal over a 500 km scale within a couple of years after the 2011 Tohoku-Oki earthquake, which is nearly 40-50% of the coseismic gravity change. It originates mostly from changes in the isotropic component corresponding to the M-rr moment tensor element. The exponential decay with rapid change in a year and gradual change afterward is a characteristic temporal pattern. Both viscoelastic relaxation and afterslip models produce reasonable agreement with the GRACE free-air gravity observation, while their Bouguer gravity patterns and seafloor vertical deformations are distinctly different. The postseismic gravity variation is best modeled by the biviscous relaxation with a transient and steady state viscosity of 10(18) and 10(19)Pas, respectively, for the asthenosphere. Our calculated higher-resolution viscoelastic relaxation model, underlying the partially ruptured elastic lithosphere, yields the localized postseismic subsidence above the hypocenter reported from the GPS-acoustic seafloor surveying.
C1 [Han, Shin-Chan; Sauber, Jeanne] NASA, Goddard Space Flight Ctr, Planetary Geodynam Lab, Greenbelt, MD 20771 USA.
[Pollitz, Fred] US Geol Survey, Menlo Pk, CA 94025 USA.
RP Han, SC (reprint author), NASA, Goddard Space Flight Ctr, Planetary Geodynam Lab, Greenbelt, MD 20771 USA.
EM shin-chan.han@nasa.gov
FU NASA's GRACE project; Earth Surface and Interior program
FX This work was supported by NASA's GRACE project and Earth Surface and
Interior program. We thank Riccardo Riva for sharing computer codes for
the normal mode analysis, Roland Burgmann and Yan Hu for sharing their
postseismic modeling and analysis, Faqi Diao for providing the finite
fault models of afterslip, and an anonymous reviewer and M. Kogan for
their constructive comments. The GRACE data for this paper are available
at http://podaac.jpl.nasa.gov/GRACE.
NR 39
TC 11
Z9 11
U1 0
U2 8
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 AUG 28
PY 2014
VL 41
IS 16
BP 5797
EP 5805
DI 10.1002/2014GL060905
PG 9
WC Geosciences, Multidisciplinary
SC Geology
GA AQ4HT
UT WOS:000342755400015
ER
PT J
AU Castle, SL
Thomas, BF
Reager, JT
Rodell, M
Swenson, SC
Famiglietti, JS
AF Castle, Stephanie L.
Thomas, Brian F.
Reager, John T.
Rodell, Matthew
Swenson, Sean C.
Famiglietti, James S.
TI Groundwater depletion during drought threatens future water security of
the Colorado River Basin
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
DE Colorado River Basin; drought; GRACE; groundwater; water management;
groundwater depletion
ID UNITED-STATES; MODEL; HYDROLOGY; SYSTEM; GRACE
AB Streamflow of the Colorado River Basin is the most overallocated in the world. Recent assessment indicates that demand for this renewable resource will soon outstrip supply, suggesting that limited groundwater reserves will play an increasingly important role in meeting future water needs. Here we analyze 9years (December 2004 to November 2013) of observations from the NASA Gravity Recovery and Climate Experiment mission and find that during this period of sustained drought, groundwater accounted for 50.1km(3) of the total 64.8km(3) of freshwater loss. The rapid rate of depletion of groundwater storage (-5.60.4km(3)yr(-1)) far exceeded the rate of depletion of Lake Powell and Lake Mead. Results indicate that groundwater may comprise a far greater fraction of Basin water use than previously recognized, in particular during drought, and that its disappearance may threaten the long-term ability to meet future allocations to the seven Basin states.
C1 [Castle, Stephanie L.; Thomas, Brian F.; Reager, John T.; Famiglietti, James S.] Univ Calif Irvine, UC Ctr Hydrol Modeling, Irvine, CA 92697 USA.
[Castle, Stephanie L.; Thomas, Brian F.; Reager, John T.; Famiglietti, James S.] Univ Calif Irvine, Dept Earth Syst Sci, Irvine, CA USA.
[Thomas, Brian F.; Reager, John T.; Famiglietti, James S.] CALTECH, NASA, Jet Prop Lab, Pasadena, CA USA.
[Rodell, Matthew] NASA, Goddard Space Flight Ctr, Hydrol Sci Lab, Greenbelt, MD 20771 USA.
[Swenson, Sean C.] Natl Ctr Atmospher Res, Climate & Global Dynam Div, Boulder, CO 80307 USA.
RP Famiglietti, JS (reprint author), Univ Calif Irvine, UC Ctr Hydrol Modeling, Irvine, CA 92697 USA.
EM jfamigli@uci.edu
RI Rodell, Matthew/E-4946-2012
OI Rodell, Matthew/0000-0003-0106-7437
FU NASA GRACE Science Team; University of California Office of the
President, Multicampus Research Programs and Initiatives; NASA
FX This research was funded by grants from the NASA GRACE Science Team and
from the University of California Office of the President, Multicampus
Research Programs and Initiatives. Jason Christensen of the U. S. Bureau
of Reclamation provided the reservoir capacities and dam releases. We
thank Q. Tang of the University of Washington for the use of the MODIS
ET data and Min-Hui Lo of the National Taiwan University for the
assistance with the GRACE validation. Access to all data sets used in
this study is available through the links provided in the main text.
Authors J.T. Reager and J.S. Famiglietti conducted some of this research
at the Jet Propulsion Laboratory, California Institute of Technology,
under a contract with NASA.
NR 42
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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 AUG 28
PY 2014
VL 41
IS 16
BP 5904
EP 5911
DI 10.1002/2014GL061055
PG 8
WC Geosciences, Multidisciplinary
SC Geology
GA AQ4HT
UT WOS:000342755400029
ER
PT J
AU Bouman, J
Fuchs, M
Ivins, E
van der Wal, W
Schrama, E
Visser, P
Horwath, M
AF Bouman, J.
Fuchs, M.
Ivins, E.
van der Wal, W.
Schrama, E.
Visser, P.
Horwath, M.
TI Antarctic outlet glacier mass change resolved at basin scale from
satellite gravity gradiometry
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
DE basin-scale ice mass change; Amundsen Sea Sector; Antarctica; satellite
gravimetry
ID ICE-SHEET; GRACE; FIELD; GOCE; GREENLAND; BALANCE; IMPACT; SHELF
AB The orbit and instrumental measurement of the Gravity Field and Steady State Ocean Circulation Explorer (GOCE) satellite mission offer the highest ever resolution capabilities for mapping Earth's gravity field from space. However, past analysis predicted that GOCE would not detect changes in ice sheet mass. Here we demonstrate that GOCE gravity gradiometry observations can be combined with Gravity Recovery and Climate Experiment (GRACE) gravity data to estimate mass changes in the Amundsen Sea Sector. This refined resolution allows land ice changes within the Pine Island Glacier (PIG), Thwaites Glacier, and Getz Ice Shelf drainage systems to be measured at respectively -677, -6312, and -559 Gt/yr over the GOCE observing period of November 2009 to June 2012. This is the most accurate pure satellite gravimetry measurement to date of current mass loss from PIG, known as the weak underbelly of West Antarctica because of its retrograde bed slope and high potential for raising future sea level.
C1 [Bouman, J.; Fuchs, M.] Deutsches Geodat Forschungsinst, Munich, Germany.
[Ivins, E.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[van der Wal, W.; Schrama, E.; Visser, P.] Delft Univ Technol, Fac Aerosp Engn, Delft, Netherlands.
[Horwath, M.] Tech Univ Munich, Inst Astron & Phys Geodasie, D-80290 Munich, Germany.
RP Bouman, J (reprint author), Deutsches Geodat Forschungsinst, Munich, Germany.
EM bouman@dgfi.badw.de
RI Bouman, Johannes/C-3521-2015
FU European Space Agency as part of the Support to Science Element (STSE)
FX This work was partially done in the context of the GOCE +
Time-Variations study, which was supported by the European Space Agency
as part of the Support to Science Element (STSE). All GOCE and GRACE
products are freely available (e.g., http://podaac.jpl.nasa.gov/GRACE,
http://icgem.gfz-potsdam.de, or http://earth.esa.int/goce). We thank
Byron Tapley and Srinivas Bettadpur for providing the extended GRACE CSR
RL05 solutions.
NR 34
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U2 18
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 AUG 28
PY 2014
VL 41
IS 16
BP 5919
EP 5926
DI 10.1002/2014GL060637
PG 8
WC Geosciences, Multidisciplinary
SC Geology
GA AQ4HT
UT WOS:000342755400031
ER
PT J
AU Field, RD
Kim, D
LeGrande, AN
Worden, J
Kelley, M
Schmidt, GA
AF Field, Robert D.
Kim, Daehyun
LeGrande, Allegra N.
Worden, John
Kelley, Maxwell
Schmidt, Gavin A.
TI Evaluating climate model performance in the tropics with retrievals of
water isotopic composition from Aura TES
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
DE climate models; convection; water isotopes; satellite retrievals;
parameterizations; tropics
ID GENERAL-CIRCULATION MODEL; BOUNDARY-LAYER; CONVECTION SCHEME;
SENSITIVITY; HDO; PARAMETERIZATIONS; CONFIGURATION; SIMULATIONS;
VARIABILITY; PROFILES
AB We evaluate the NASA Goddard Institute for Space Studies ModelE2 general circulation model over the tropics against water isotope (HDO/H2O) retrievals from the Aura Tropospheric Emission Spectrometer. Observed isotopic distributions are distinct from other observable quantities and can therefore act as an independent constraint. We perform a small ensemble of simulations with physics perturbations to the cumulus and planetary boundary layer schemes. We examine the degree to which model-data agreement could be used to constrain a select group of internal processes in the model, namely, condensate evaporation, entrainment strength, and updraft mass flux. All are difficult to parameterize but exert strong influence over model performance. We find that the water isotope composition is more sensitive to physics changes than precipitation, temperature, or relative humidity in the lower and upper tropical tropospheres. Among the processes considered, this is most closely, and fairly exclusively, related to midtropospheric entrainment strength. Our study indicates that water isotope observations could provide useful constraints on model parameterizations.
C1 [Field, Robert D.; LeGrande, Allegra N.; Kelley, Maxwell; Schmidt, Gavin A.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
[Field, Robert D.] Columbia Univ, Dept Appl Phys & Appl Math, New York, NY USA.
[Kim, Daehyun] Univ Washington, Dept Atmospher Sci, Seattle, WA 98195 USA.
[Worden, John] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Kelley, Maxwell] Trinnovim LLC, New York, NY USA.
RP Field, RD (reprint author), NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
EM rf2426@columbia.edu
RI Schmidt, Gavin/D-4427-2012
OI Schmidt, Gavin/0000-0002-2258-0486
FU NASA Postdoctoral Program; NASA [NNX13AK46G, NNX13AM18G]; Korea
Meteorological Administration Research and Development Program [CATER
2013-3142]; National Aeronautics and Space Administration
FX R.F. was supported by the NASA Postdoctoral Program and NASA grant
NNX13AK46G and D. K. by NASA grant NNX13AM18G and the Korea
Meteorological Administration Research and Development Program under
grant CATER 2013-3142. 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.
Resources supporting this work were provided by the NASA High-End
Computing Program through the NASA Center for Climate Simulation at the
Goddard Space Flight Center. All data used in the paper can be obtained
from the authors. The authors thank three anonymous reviewers for their
constructive comments.
NR 45
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Z9 9
U1 1
U2 12
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 AUG 28
PY 2014
VL 41
IS 16
BP 6030
EP 6036
DI 10.1002/2014GL060572
PG 7
WC Geosciences, Multidisciplinary
SC Geology
GA AQ4HT
UT WOS:000342755400045
ER
PT J
AU Fortenberry, RC
Huang, XC
Crawford, TD
Lee, TJ
AF Fortenberry, Ryan C.
Huang, Xinchuan
Crawford, T. Daniel
Lee, Timothy J.
TI Quartic Force Field Rovibrational Analysis of Protonated Acetylene,
C2H3+, and Its Isotopologues
SO JOURNAL OF PHYSICAL CHEMISTRY A
LA English
DT Article
ID FUNDAMENTAL VIBRATIONAL FREQUENCIES; SPECTROSCOPIC CONSTANTS;
INFRARED-SPECTROSCOPY; WAVE-FUNCTIONS; LINEAR C3H3+; BASIS-SETS;
ENERGIES; CYCLOPROPENYLIDENE; MOLECULES; HYDROGEN
AB Protonated acetylene, C2H3+, is among the simplest carbocations. Comprehensive experimental or highly accurate computational spectroscopic data is lacking for this system due to its inherent complexities. Utilizing state-of-the-art quartic force fields (QFFs), the spectroscopic constants and fundamental vibrational frequencies are provided in this work for the nonclassical, bridged, cyclic global minimum. The rotational constants match experiment to better than 0.1%, and the computed nu(2) antisymmetric HCCH stretch is less than 3.0 cm(-1) different from experiment. Hence, the rovibrational spectroscopic data provided herein for c-C2H3+ and its deuterated isotopologues enrich the chemical understanding of this system. Unfortunately, the same rovibrational spectroscopic data is not as trustworthy for the classical, linear form of protonated acetylene due to the shallow well in which it resides on the potential energy surface. However, spectroscopic data are provided for this isomer in the Supporting Information to enhance future studies.
C1 [Fortenberry, Ryan C.] Georgia So Univ, Dept Chem, Statesboro, GA 30460 USA.
[Fortenberry, Ryan C.; Huang, Xinchuan] SETI Inst, Mountain View, CA 94043 USA.
[Crawford, T. Daniel] Virginia Tech, Dept Chem, Blacksburg, VA 24061 USA.
[Fortenberry, Ryan C.; Lee, Timothy J.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
RP Fortenberry, RC (reprint author), Georgia So Univ, Dept Chem, Statesboro, GA 30460 USA.
EM rfortenberry@georgiasouthern.edu; Timothy.J.Lee@nasa.gov
RI Lee, Timothy/K-2838-2012; HUANG, XINCHUAN/A-3266-2013; Crawford,
Thomas/A-9271-2017
OI Crawford, Thomas/0000-0002-7961-7016
FU Georgia Southern University; NASA; National Science Foundation (NSF)
[CHE-1058420]; NSF Multi-User Chemistry Research Instrumentation and
Facility (CRIF:MU) Award [CHE-0741927]; NASA [12-APRA12-0107]; NASA/SETI
Institute [NNX12AG96A]; NASA's Laboratory Astrophysics "Carbon in the
Galaxy" Consortium Grant [NNH10ZDA001N]
FX Georgia Southern University provided start-up funds, and the NASA
Postdoctoral Program administered by Oak Ridge Associated Universities
through a contract with NASA financially supported the work performed by
R.C.F. T.D.C. was supported by National Science Foundation (NSF) Award
CHE-1058420 and by NSF Multi-User Chemistry Research Instrumentation and
Facility (CRIF:MU) Award CHE-0741927, which provided the employed
computer hardware. T.J.L., R.C.F., and X.H. gratefully acknowledge
funding from NASA Grant 12-APRA12-0107. X.H. was funded by NASA/SETI
Institute Cooperative Agreement NNX12AG96A. Support from NASA's
Laboratory Astrophysics "Carbon in the Galaxy" Consortium Grant
(NNH10ZDA001N) is acknowledged by T.J.L., R.C.F., and X.H. The figures
were created using the CheMVP program developed at the University of
Georgia's Center for Computational Quantum Chemistry.
NR 47
TC 22
Z9 22
U1 1
U2 10
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 AUG 28
PY 2014
VL 118
IS 34
BP 7034
EP 7043
DI 10.1021/jp506441g
PG 10
WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical
SC Chemistry; Physics
GA AO2BR
UT WOS:000341121000035
PM 25076406
ER
PT J
AU Li, JLF
Forbes, RM
Waliser, DE
Stephens, G
Lee, S
AF Li, J. -L. F.
Forbes, R. M.
Waliser, D. E.
Stephens, G.
Lee, Seungwon
TI Characterizing the radiative impacts of precipitating snow in the ECMWF
Integrated Forecast System global model
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
ID LARGE-SCALE MODELS; PARTICLE-SIZE DISTRIBUTIONS; CLIMATE MODELS;
ACCURATE PARAMETERIZATION; MACROSCOPIC BEHAVIOR; ATMOSPHERE RADIATION;
CLOUD-MICROPHYSICS; CUMULUS ENSEMBLES; CIRRUS CLOUDS; SENSITIVITY
AB Global weather and climate models often exclude the effects of precipitating hydrometeors and convective core mass on radiative fluxes. In particular, many models split the ice phase into separate "cloud ice" and "snow" categories representing the smaller and larger ice particles, respectively; a separation that is generally not well defined in observations. A version of the European Centre for Medium-Range Weather Forecasts (ECMWF) global numerical weather prediction model which includes the radiative effects of cloud liquid, cloud ice, and precipitating snow is used to investigate the impact of including and excluding the radiative effects of the precipitating snow category. The results show that exclusion of precipitating snow in the radiation calculations leads to differences in the shortwave and longwave radiative fluxes of 5-15 Wm(-2) in strongly precipitating and convective areas. These differences are of the same order of magnitude as the systematic errors in the model compared to satellite observations. Corresponding biases in the radiative heating profiles are on the order of 0.15 K d(-1). The results imply that precipitating snow should be included in the radiative calculations in all weather and climate models in the context of improving model fidelity and reducing compensating errors.
C1 [Li, J. -L. F.; Waliser, D. E.; Stephens, G.; Lee, Seungwon] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
[Forbes, R. M.] ECMWF, Reading, Berks, England.
RP Li, JLF (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
EM Juilin.F.Li@jpl.nasa.gov
FU Jet Propulsion Laboratory, California Institute of Technology
[NNH12ZDA001N ROSES 2012]; ATMOS COMP [NNH12ZDA001N-CCST]
FX We thank Justin Stachnik and Terry Kubar at JPL for useful comments. The
contributions by D. E. W., S. L., and J.L.L. to this study were carried
out on behalf of the Jet Propulsion Laboratory, California Institute of
Technology, under contracts of NNH12ZDA001N ROSES 2012, Earth Science
Program, the Modeling, Analysis, and Prediction (MAP) and ATMOS COMP
2013 (NNH12ZDA001N-CCST) with the National Aeronautics and Space
Administration (NASA). The observations from the CloudSat radar
(http://www.cloudsat.cira.colostate.edu/) and CERES Energy Balanced and
Filled (CERES-EBAF) and corresponding surface flux radiation products
constrained by TOA CERES-EBAF adjustments can be found at
http://ceres.larc.nasa.gov/cmip5_data.php.
NR 39
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U1 1
U2 10
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-897X
EI 2169-8996
J9 J GEOPHYS RES-ATMOS
JI J. Geophys. Res.-Atmos.
PD AUG 27
PY 2014
VL 119
IS 16
BP 9626
EP 9637
DI 10.1002/2014JD021450
PG 12
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA AP3RF
UT WOS:000341994000002
ER
PT J
AU Frith, SM
Kramarova, NA
Stolarski, RS
McPeters, RD
Bhartia, PK
Labow, GJ
AF Frith, S. M.
Kramarova, N. A.
Stolarski, R. S.
McPeters, R. D.
Bhartia, P. K.
Labow, G. J.
TI Recent changes in total column ozone based on the SBUV Version 8.6
Merged Ozone Data Set
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
ID QUASI-BIENNIAL OSCILLATION; ABSORPTION CROSS-SECTIONS; STRATOSPHERIC
CHLORINE; UV SPECTROSCOPY; TEMPERATURE; TRENDS; CALIBRATION; INSTRUMENT;
ALGORITHM; RECORD
AB The Solar Backscatter Ultraviolet (SBUV) Merged Ozone Data Set (MOD) provides the longest available satellite-based time series of profile and total ozone from a single instrument type. The data span a 44 year period from 1970 to 2013 (except a 5 year gap in the 1970s). Data from nine independent SBUV-type instruments are included in the record, one of which is still operating. Although modifications in instrument design were made in the evolution from the Nimbus-4 Backscattered Ultraviolet instrument to the modern SBUV(/2) model, the basic principles of the measurement technique and retrieval algorithm remain the same, lending consistency to this record compared to those based on measurements using different instrument types. Nevertheless, each instrument has specific characteristics, and known anomalies must be incorporated in the MOD uncertainty estimates. In this study we describe the latest version of the MOD data set based on SBUV data processed using the Version 8.6 algorithm. We assess the measurement consistency across instruments and use this information to assign a drift uncertainty to the MOD. We then fit a multiple regression model to the MOD time series alternately using Equivalent Effective Stratospheric Chlorine (EESC) or linear trend fits over varying time series segments to analyze trends. Regression results indicate a statistically significant positive trend in total ozone outside the tropics based on the EESC proxy fit to the full record, but a linear trend fit to the last 13 years of data does not yield a statistically significant ozone increase.
C1 [Frith, S. M.; Kramarova, N. A.; Labow, G. J.] Sci Syst & Applicat Inc, Lanham, MD 20706 USA.
[Stolarski, R. S.] Johns Hopkins Univ, Dept Earth & Planetary Sci, Baltimore, MD 21218 USA.
[McPeters, R. D.; Bhartia, P. K.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Frith, SM (reprint author), Sci Syst & Applicat Inc, Lanham, MD 20706 USA.
EM stacey.m.frith@nasa.gov
RI Stolarski, Richard/B-8499-2013; McPeters, Richard/G-4955-2013;
Kramarova, Natalya/D-2270-2014
OI Stolarski, Richard/0000-0001-8722-4012; McPeters,
Richard/0000-0002-8926-8462; Kramarova, Natalya/0000-0002-6083-8548
FU NASA [NNG12HP08C]
FX The authors would like to acknowledge the SBUV instrument team members
for their work producing the Version 8.6 SBUV data. SBUV Version 8.6
Level 2 and Level 3 data can be accessed from the "Instruments" tab on
the MOD website at
http://acdb-ext.gsfc.nasa.gov/Data_services/merged/index.html.
Ground-based data are publicly available through the World Ozone and UV
Data Center (WOUDC). The GTO merged ozone record used in this work was
created within the framework of the ESA Climate Change Initiative
program and is available from the ozone CCI website
(http://www.esa-ozone-cci.org/). Data sources for proxies used in the
regression analysis are provided in the text (Section 2.3). We also
thank the three anonymous reviews for their comments and constructive
improvements to this manuscript. S. M. Frith is supported under NASA
Contract NNG12HP08C.
NR 47
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U1 1
U2 19
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 AUG 27
PY 2014
VL 119
IS 16
BP 9735
EP 9751
DI 10.1002/2014JD021889
PG 17
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA AP3RF
UT WOS:000341994000010
ER
PT J
AU Russell, PB
Kacenelenbogen, M
Livingston, JM
Hasekamp, OP
Burton, SP
Schuster, GL
Johnson, MS
Knobelspiesse, KD
Redemann, J
Ramachandran, S
Holben, B
AF Russell, Philip B.
Kacenelenbogen, Meloe
Livingston, John M.
Hasekamp, Otto P.
Burton, Sharon P.
Schuster, Gregory L.
Johnson, Matthew S.
Knobelspiesse, Kirk D.
Redemann, Jens
Ramachandran, S.
Holben, Brent
TI A multiparameter aerosol classification method and its application to
retrievals from spaceborne polarimetry
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
ID OPTICAL-PROPERTIES; CARBONACEOUS AEROSOLS; ABSORPTION PROPERTIES; LIDAR
MEASUREMENTS; CENTRAL MEXICO; AERONET; INSTRUMENT; POLARIZATION;
CLIMATOLOGY; INTENSITY
AB Classifying observed aerosols into types (e. g., urban-industrial, biomass burning, mineral dust, maritime) helps to understand aerosol sources, transformations, effects, and feedback mechanisms; to improve accuracy of satellite retrievals; and to quantify aerosol radiative impacts on climate. The number of aerosol parameters retrieved from spaceborne sensors has been growing, from the initial aerosol optical depth (AOD) at one or a few wavelengths to a list that now includes AOD, complex refractive index, single scattering albedo (SSA), and depolarization of backscatter, each at several wavelengths, plus several particle size and shape parameters. Making optimal use of these varied data products requires objective, multidimensional analysis methods. We describe such a method, which makes explicit use of uncertainties in input parameters. It treats an N-parameter retrieved data point and its N-dimensional uncertainty as an extended data point, E. It then uses a modified Mahalanobis distance, D-EC, to assign an observation to the class (cluster) C that has minimum DEC from the point. We use parameters retrieved from the Aerosol Robotic Network (AERONET) to define seven prespecified clusters (pure dust, polluted dust, urban-industrial/developed economy, urban-industrial/developing economy, dark biomass smoke, light biomass smoke, and pure marine), and we demonstrate application of the method to a 5 year record of retrievals from the spaceborne Polarization and Directionality of the Earth's Reflectances 3 (POLDER 3) polarimeter over the island of Crete, Greece. Results show changes of aerosol type at this location in the eastern Mediterranean Sea, which is influenced by a wide variety of aerosol sources.
C1 [Russell, Philip B.; Johnson, Matthew S.; Knobelspiesse, Kirk D.; Redemann, Jens] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Kacenelenbogen, Meloe] Bay Area Environm Res Inst, Sonoma, CA USA.
[Livingston, John M.] SRI Int, Menlo Pk, CA 94025 USA.
[Hasekamp, Otto P.] SRON Netherlands Inst Space Res, Utrecht, Netherlands.
[Burton, Sharon P.; Schuster, Gregory L.] NASA, Langley Res Ctr, Hampton, VA 23665 USA.
[Ramachandran, S.] Phys Res Lab, Ahmadabad 380009, Gujarat, India.
[Holben, Brent] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Russell, PB (reprint author), NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
EM Philip.B.Russell@nasa.gov
RI Knobelspiesse, Kirk/S-5902-2016
OI Knobelspiesse, Kirk/0000-0001-5986-1751
FU NASA Atmospheric Composition Modeling and Analysis Program (ACMAP); NASA
Glory Science Team funding
FX This research was supported by the NASA Atmospheric Composition Modeling
and Analysis Program (ACMAP) and by NASA Glory Science Team funding. We
appreciate the efforts of the AERONET principal investigators for
obtaining, processing, documenting, and disseminating their respective
data sets. The GEOS-5 data used in this study/project have been provided
by the Global Modeling and Assimilation Office (GMAO) at NASA Goddard
Space Flight Center. We appreciate the comments of three anonymous
reviewers that have helped us to improve the paper. AERONET data used in
this paper were obtained from
http://aeronet.gsfc.nasa.gov/new_web/data.html. Relative humidity
profiles were obtained from
http://www-calipso.larc.nasa.gov/resources/calipso_users_guide/data_-sum
maries/profile_data.php#relative_-humidity. POLDER data are available
from Otto Hasekamp, SRON Netherlands Institute for Space Research,
Utrecht, Netherlands, O.P. Hasekamp@sron.nl.
NR 68
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Z9 17
U1 1
U2 18
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 AUG 27
PY 2014
VL 119
IS 16
BP 9838
EP 9863
DI 10.1002/2013JD021411
PG 26
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA AP3RF
UT WOS:000341994000016
ER
PT J
AU Bi, JR
Huang, JP
Hu, ZY
Holben, BN
Guo, ZQ
AF Bi, Jianrong
Huang, Jianping
Hu, Zhiyuan
Holben, B. N.
Guo, Zhiqiang
TI Investigating the aerosol optical and radiative characteristics of heavy
haze episodes in Beijing during January of 2013
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
ID SKY RADIANCE MEASUREMENTS; AIR-POLLUTION; CHEMICAL-PROPERTIES; SOLAR
IRRADIANCE; DUST AEROSOLS; CHINA; PM2.5; AERONET; CLIMATE; URBAN
AB Several heavy atmospheric haze pollution episodes occurred over eastern and northern China during January of 2013. The pollution covered more than 100 km(2) and caused serious impacts on environmental quality, human health, and transportation. In this study, we characterize aerosol microphysical, optical, and radiative characteristics using a combination of ground-based Sun/sky radiometer retrievals and a radiative transfer model. Our results show that during about half of the total number of days, daily PM2.5 and PM10 concentrations are larger than 100 mu g/m(3), with maxima of 462 and 433 mu g/m(3), respectively, during the haze events. Fine-mode (PM2.5) particles dominated the aerosol size during the episodes. The volume size distribution and median radius of fine-mode particles generally increase as aerosol optical depth at 440 nm (AOD(440)) increases. The median effective radius of fine-mode particles increases from 0.15 mu m at low AOD value (AOD(440)similar to 0.3) to a radius of 0.25-0.30 mu m at high AOD value (AOD(440) >= 1.0). The daily mean single-scattering albedo (SSA), imaginary part of refractive index (RI), and asymmetry factor display pronounced spectral behaviors. The overall mean SSA(440) and SSA(675) are 0.892 and 0.905, respectively. The corresponding RI440 and RI675 are 0.016 and 0.011, respectively. This indicates that a significant amount of absorption occurred under the haze event in Beijing during January 2013. Approximately half of the incident solar radiation energy went into heating the atmosphere as a result of strong aerosol loading and absorption. The daily averaged heating rate in the haze particle layer (0-3.2 km) varies from 0.12 to 0.81 K/day in Beijing, which might exert profound impact on the atmospheric thermodynamic and dynamical structures and cloud development, which should be further studied.
C1 [Bi, Jianrong; Huang, Jianping; Hu, Zhiyuan] Lanzhou Univ, Minist Educ, Key Lab Semiarid Climate Change, Lanzhou 730000, Peoples R China.
[Bi, Jianrong; Huang, Jianping; Hu, Zhiyuan] Lanzhou Univ, Coll Atmospher Sci, Lanzhou 730000, Peoples R China.
[Holben, B. N.] NASA, Biospher Sci Branch, GSFC, Greenbelt, MD USA.
[Guo, Zhiqiang] Baoding City Bur Meteorol, Baoding, Peoples R China.
RP Huang, JP (reprint author), Lanzhou Univ, Minist Educ, Key Lab Semiarid Climate Change, Lanzhou 730000, Peoples R China.
EM hjp@lzu.edu.cn
RI Xiongfei, Zhao/G-7690-2015
FU Lanzhou University through 985 Program; National Basic Research Program
of China [2012CB955302, 2013CB955802]; National Science Foundation of
China [41305025, 41175134]; Fundamental Research Funds for the Central
Universities [lzujbky-2013-207, lzujbky-2013-ct05]; Developmental
Program of Changjiang Scholarship and Research Team [IRT1018]
FX SACOL was sponsored by Lanzhou University through 985 Program. This work
was jointly supported by the National Basic Research Program of China
(2012CB955302 and 2013CB955802), and National Science Foundation of
China under grant 41305025 and 41175134. The Fundamental Research Funds
for the Central Universities lzujbky-2013-207 and lzujbky-2013-ct05, and
the Developmental Program of Changjiang Scholarship and Research Team
(IRT1018). We thank the GSFC/NASA AERONET group for processing the
AERONET data (http://aeronet.gsfc.nasa.gov). The authors would like to
express special thanks to the principal investigators at Beijing-CAMS
site (Huizheng Che, Chinese Academy of Meteorological Sciences, China
Meteorological Administration), Beijing site (Hongbin Chen, Institute of
Atmospheric Physics, Chinese Academy of Sciences), and Beijing_RADI site
(Zhengqiang Li, Institute of Remote Sensing and Digital Earth of Chinese
Academy of Sciences) together with their staff for establishing and
maintaining the instruments. We are grateful to the Chinese
Environmental Protection Bureau and the U. S. Embassy to provide the
daily mean data of PM2.5 and PM10 concentrations
in Beijing. We appreciate the MODIS and TOMS teams for supplying the
satellite data. We would also like to thank all anonymous reviewers for
their constructive and insightful comments.
NR 60
TC 17
Z9 19
U1 3
U2 77
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 AUG 27
PY 2014
VL 119
IS 16
BP 9884
EP 9900
DI 10.1002/2014JD021757
PG 17
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA AP3RF
UT WOS:000341994000018
ER
PT J
AU Lee, SS
Feingold, G
McComiskey, A
Yamaguchi, T
Koren, I
Martins, JV
Yu, HB
AF Lee, Seoung Soo
Feingold, Graham
McComiskey, Allison
Yamaguchi, Takanobu
Koren, Ilan
Martins, J. Vanderlei
Yu, Hongbin
TI Effect of gradients in biomass burning aerosol on shallow cumulus
convective circulations
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
ID BLACK CARBON AEROSOLS; BOUNDARY-LAYER; WRF MODEL; PART I; CLOUDS;
SIMULATIONS; CLIMATE; AMAZON; SMOKE; SENSITIVITY
AB This study examines the effect of spatial gradients in biomass burning (BB) aerosol on mesoscale circulations and clouds in the Amazon through high-resolution numerical modeling over areas of 30 km to 60 km. Inhomogeneous horizontal distribution of BB aerosol results in differential surface heat fluxes and radiative heating of the air, which generates circulation patterns that strongly influence cloud formation. The influence on air circulation and cumulus cloud formation depends on the BB aerosol loading, its vertical location, and the width of the plume. Plumes that reside at higher altitudes (similar to 1.5 km altitude) produce monotonic responses to aerosol loading whereas the response to plumes close to the surface changes nonmonotonically with plume width and aerosol loading. Sensitivity tests highlight the importance of interactive calculations of surface latent and heat fluxes with a coupled land surface model. In the case of the plume residing at higher altitude, failure to use interactive fluxes results in a reversal of the circulation whereas for the plume residing nearer the surface, the interactive surface model weakens the circulation. The influence of the BB aerosol on heating patterns, circulations, surface fluxes, and resultant cloud amount prevails over the BB aerosol-cloud microphysical influences.
C1 [Lee, Seoung Soo; Feingold, Graham; McComiskey, Allison; Yamaguchi, Takanobu] NOAA, Chem Sci Div, Earth Syst Res Lab, Boulder, CO 80305 USA.
[Lee, Seoung Soo; McComiskey, Allison; Yamaguchi, Takanobu] Univ Colorado, Cooperat Inst Res Environm Sci, Boulder, CO 80309 USA.
[Koren, Ilan] Weizmann Inst Sci, Dept Earth & Planetary Sci, IL-76100 Rehovot, Israel.
[Martins, J. Vanderlei] Univ Maryland Baltimore Cty, Dept Phys, Baltimore, MD 21228 USA.
[Yu, Hongbin] Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20742 USA.
[Yu, Hongbin] NASA, Goddard Space Flight Ctr, Climate & Radiat Lab, Greenbelt, MD 20771 USA.
RP Lee, SS (reprint author), NOAA, Chem Sci Div, Earth Syst Res Lab, Boulder, CO 80305 USA.
EM cumulss@gmail.com
RI Manager, CSD Publications/B-2789-2015; Feingold, Graham/B-6152-2009;
Koren, Ilan/K-1417-2012; Yamaguchi, Takanobu/H-9169-2013; Yu,
Hongbin/C-6485-2008
OI Koren, Ilan/0000-0001-6759-6265; Yamaguchi,
Takanobu/0000-0001-8059-0757; Yu, Hongbin/0000-0003-4706-1575
FU NASA's IDS program; NOAA's Climate Goal Program
FX The authors thank NASA's IDS program administered by Hal Maring and
NOAA's Climate Goal Program for supporting this work. NOAA's HPCC is
acknowledged for computing support. Data used in this study can be
obtained by contacting Seoung Soo Lee (Seoung.Soo.Lee@noaa.gov).
NR 44
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U1 3
U2 28
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 AUG 27
PY 2014
VL 119
IS 16
BP 9948
EP 9964
DI 10.1002/2014JD021819
PG 17
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA AP3RF
UT WOS:000341994000022
ER
PT J
AU Cooper, M
Martin, RV
Wespes, C
Coheur, PF
Clerbaux, C
Murray, LT
AF Cooper, Matthew
Martin, Randall V.
Wespes, Catherine
Coheur, Pierre-Francois
Clerbaux, Cathy
Murray, Lee T.
TI Tropospheric nitric acid columns from the IASI satellite instrument
interpreted with a chemical transport model: Implications for
parameterizations of nitric oxide production by lightning
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
ID PACIFIC EXPLORATORY MISSION; ATMOSPHERIC-CHEMISTRY; OZONE PRODUCTION;
NITROGEN-OXIDES; AIRBORNE MEASUREMENTS; TROPICAL PACIFIC; NOX
PRODUCTION; GEOS-CHEM; DISTRIBUTIONS; EMISSIONS
AB This paper interprets tropical tropospheric nitric acid columns from the Infrared Atmospheric Sounding Interferometer (IASI) satellite instrument with a global chemical transport model (GEOS-Chem). GEOS-Chemand IASI columns generally agree over the tropical ocean to within 10%. However, the GEOS-Chem simulation underestimates IASI nitric acid over Southeast Asia by a factor of 2. The regional nitric acid bias is confirmed by comparing the GEOS-Chem simulation with additional satellite (High Resolution Dynamics Limb Sounder, Atmospheric Chemistry Experiment Fourier Transform Spectrometer) and aircraft (Pacific Exploratory Mission (PEM)-Tropics A and PEM-West B) observations of the middle and upper troposphere. This bias appears to be driven by the lightning NOx parameterization, both in terms of the magnitude of the NOx source and the ozone production efficiency of concentrated lightning NOx plumes. We tested a subgrid lightning plume parameterization and found that an ozone production efficiency of 15 mol/mol in lightning plumes over Southeast Asia in conjunction with an additional 0.5 Tg N would reduce the regional nitric acid bias from 92% to 6% without perturbing the rest of the tropics. Other sensitivity studies such as modified NOx yield per flash, increased altitude of lightning NOx emissions, decreased convective mass flux, or increased scavenging of nitric acid required unrealistic changes to reduce the bias.
C1 [Cooper, Matthew; Martin, Randall V.] Dalhousie Univ, Dept Phys & Atmospher Sci, Halifax, NS, Canada.
[Martin, Randall V.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Wespes, Catherine; Coheur, Pierre-Francois; Clerbaux, Cathy] Univ Libre Bruxelles, Brussels, Belgium.
[Clerbaux, Cathy] Univ Paris 06, Sorbonne Univ, Paris, France.
[Clerbaux, Cathy] Univ Versailles St Quentin, Paris, France.
[Clerbaux, Cathy] LATMOS IPSL, CNRS INSU, Paris, France.
[Murray, Lee T.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
[Murray, Lee T.] Columbia Univ, Lamont Doherty Earth Observ, New York, NY USA.
RP Cooper, M (reprint author), Dalhousie Univ, Dept Phys & Atmospher Sci, Halifax, NS, Canada.
EM cooperm2@dal.ca
RI Chem, GEOS/C-5595-2014; Murray, Lee/F-2296-2014; Martin,
Randall/C-1205-2014; clerbaux, cathy/I-5478-2013
OI Murray, Lee/0000-0002-3447-3952; Martin, Randall/0000-0003-2632-8402;
FU Natural Sciences and Engineering Research Council of Canada; Belgian
State Federal Office for Scientific, Technical and Cultural Affairs;
European Space Agency (ESA Prodex IASI.Flow); EUMETSAT (O3MSAF)
FX IASI HNO3 data are available on request by contacting P.-F
Coheur. IASI CO data were provided by LATMOS/CNRS and ULB and are
available online at the Ether database at http://www.pole-ether.fr/.
HIRDLS data products are available online at NASA's Goddard Earth
Sciences Data and Information Services Center. ACE-FTS data are
available on request by contacting the ACE Science Team at
info@scisat.ca. Aircraft data from PEM West and PEM-Tropics campaigns
are made available online at NASA's Global Tropospheric Experiment
webpage at http://www-gte.larc.nasa.gov/gte_fld.htm. SHADOZ ozonesonde
measurements are available online at http://croc.gsfc.nasa.gov/shadoz/.
Information on accessing GEOS-Chem code can be found online at
geos-chem.org. This work was supported by the Natural Sciences and
Engineering Research Council of Canada. P.-F. Coheur and C. Wespes are,
respectively, Senior Research Associate and Postdoctoral Researcher with
F.R.S.-FNRS. The research in Belgium was also funded by the Belgian
State Federal Office for Scientific, Technical and Cultural Affairs and
the European Space Agency (ESA Prodex IASI.Flow), as well as by EUMETSAT
(O3MSAF).
NR 62
TC 5
Z9 5
U1 0
U2 27
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 AUG 27
PY 2014
VL 119
IS 16
BP 10068
EP 10079
DI 10.1002/2014JD021907
PG 12
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA AP3RF
UT WOS:000341994000030
ER
PT J
AU Moriarty, JA
Haskins, JB
AF Moriarty, John A.
Haskins, Justin B.
TI Efficient wide-range calculation of free energies in solids and liquids
using reversible-scaling molecular dynamics
SO PHYSICAL REVIEW B
LA English
DT Article
ID STRUCTURAL PHASE-STABILITY; EQUATION-OF-STATE; TRANSITION-METALS;
INTERATOMIC POTENTIALS; HIGH-PRESSURE; ATOMISTIC SIMULATION; TANTALUM;
MAGNESIUM; THERMODYNAMICS; ALUMINUM
AB We elaborate a novel and efficient method to obtain multiphase Helmholtz free energies from molecular dynamics (MD) simulations over wide ranges of volume and temperature in materials that can be described by temperature-independent ion forces, with both higher accuracy and order-of-magnitude cost savings compared to direct thermodynamic-integration techniques. Our method leverages and significantly extends the technique of reversible-scaling molecular dynamics (RSMD) proposed by de Koning et al. [Phys. Rev. Lett. 83, 3973 (1999)], which allows a free-energy difference in a given phase at constant volume to be calculated as a function of temperature from a single MD simulation. In mechanically stable solid phases, our approach carefully combines quasiharmonic lattice dynamics at low temperatures with an accurate and fully isolated RSMD simulation of the anharmonic vibrational free energy at high temperatures to produce a seamless free energy from zero temperature to above melt along constant-volume isochores. In the liquid, we combine a unique calculation of the free energy along a high-temperature reference isotherm with isochoric RSMD simulations from that temperature to below melt. In metastable solid phases that are mechanically unstable at low temperature, we use two-phase MD melt simulations together with the liquid free energy to obtain the solid free energy along the solidus melt line and then perform isochoric RSMD simulations to temperatures above and below that point. While our free-energy method is general, we have specifically adapted it here to the case of metals in which the ion forces are well described by model generalized pseudopotential theory (MGPT) multi-ion interatomic potentials, and additive electron-thermal free-energy contributions can be included. Then using refined Ta6.8x MGPT potentials, we have converged total free energies and their components to very high and unprecedented sub-milli-Rydberg (mRy) numerical accuracy in the stable-bcc, liquid, and metastable-fcc phases of tantalum for volumes ranging from up to 26% expansion to nearly twofold compression and for temperatures to 25 000 K. In turn, we have successfully used the free energies so obtained to calculate physically accurate thermodynamic properties and gain new insight into their behavior, including sensitive thermodynamic derivatives, bcc and fcc melt curves, and a multiphase equation of state for tantalum (Ta) over the same temperature range and for pressures as high as 600 GPa. We show that the anharmonic free-energy component in the bcc solid, although only 1-5 mRy in magnitude for Ta, can have a significant (15%-20%) effect on thermal expansivity, the Gruneisen parameter, and melt temperatures. We further show that the electron-thermal free-energy component can similarly impact the specific heat and thermal expansivity in both the solid and the liquid, while only minimally affecting (to <= 3%) the bcc and fcc melt curves.
C1 [Moriarty, John A.] Lawrence Livermore Natl Lab, Condensed Matter & Mat Div, Livermore, CA 94551 USA.
[Haskins, Justin B.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
RP Moriarty, JA (reprint author), Lawrence Livermore Natl Lab, Condensed Matter & Mat Div, Livermore, CA 94551 USA.
FU U.S. Department of Energy by Lawrence Livermore National Laboratory
[DE-AC52-07NA27344]; DOE SciDAC [DE-FC02-06ER25788]
FX This work was performed under the auspices of the U.S. Department of
Energy by Lawrence Livermore National Laboratory under Contract No.
DE-AC52-07NA27344. J.B.H. acknowledges support as a summer student at
LLNL in 2011 from DOE SciDAC Grant No. DE-FC02-06ER25788, during which
time some of this work was begun.
NR 59
TC 2
Z9 2
U1 2
U2 23
PU AMER PHYSICAL SOC
PI COLLEGE PK
PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA
SN 1098-0121
EI 1550-235X
J9 PHYS REV B
JI Phys. Rev. B
PD AUG 22
PY 2014
VL 90
IS 5
AR 054113
DI 10.1103/PhysRevB.90.054113
PG 19
WC Physics, Condensed Matter
SC Physics
GA AO3NI
UT WOS:000341237600002
ER
PT J
AU Stecker, FW
Scully, ST
AF Stecker, Floyd W.
Scully, Sean T.
TI Propagation of superluminal PeV IceCube neutrinos: A high energy
spectral cutoff or new constraints on Lorentz invariance violation
SO PHYSICAL REVIEW D
LA English
DT Article
ID GAMMA-RAYS; RADIATION; GALAXIES
AB The IceCube observation of cosmic neutrinos with E-nu > 60 TeV, most of which are likely of extragalactic origin, allows one to severely constrain Lorentz invariance violation (LIV) in the neutrino sector, allowing for the possible existence of superluminal neutrinos. The subsequent neutrino energy loss by vacuum e(+)e(-) pair emission (VPE) is strongly dependent on the strength of LIV. In this paper we explore the physics and cosmology of superluminal neutrino propagation. We consider a conservative scenario for the redshift distribution of neutrino sources. Then by propagating a generic neutrino spectrum, using Monte Carlo techniques to take account of energy losses from both VPE and redshifting, we obtain the best present constraints on LIV parameters involving neutrinos. We find that delta(nu e) = delta(nu) - delta(e) <= 5.2 x 10(-21). Taking delta(e) <= 5 x 10(-21), we then obtain an upper limit on the superluminal velocity fraction for neutrinos alone of 1.0 x 10(-21). Interestingly, by taking delta(nu e) = 5.2 x 10(-21), we obtain a cutoff in the predicted neutrino spectrum above 2 PeV that is consistent with the lack of observed neutrinos at those energies, and particularly at the Glashow resonance energy of 6.3 PeV. Thus, such a cutoff could be the result of neutrinos being slightly superluminal, with delta(nu) being (0.5 to 1.0) x 10(-20).
C1 [Stecker, Floyd W.] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA.
[Scully, Sean T.] James Madison Univ, Dept Phys, Harrisonburg, VA 22807 USA.
RP Stecker, FW (reprint author), NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA.
EM Floyd.W.Stecker@nasa.gov
NR 39
TC 14
Z9 14
U1 0
U2 0
PU AMER PHYSICAL SOC
PI COLLEGE PK
PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA
SN 1550-7998
EI 1550-2368
J9 PHYS REV D
JI Phys. Rev. D
PD AUG 22
PY 2014
VL 90
IS 4
AR 043012
DI 10.1103/PhysRevD.90.043012
PG 5
WC Astronomy & Astrophysics; Physics, Particles & Fields
SC Astronomy & Astrophysics; Physics
GA AO3OZ
UT WOS:000341243600002
ER
PT J
AU Aasi, J
Abbott, BP
Abbott, R
Abbott, T
Abernathy, MR
Accadia, T
Acernese, F
Ackley, K
Adams, C
Adams, T
Addesso, P
Adhikari, RX
Affeldt, C
Agathos, M
Aggarwal, N
Aguiar, OD
Ain, A
Ajith, P
Alemic, A
Allen, B
Allocca, A
Amariutei, D
Andersen, M
Anderson, R
Anderson, SB
Anderson, WG
Arai, K
Araya, MC
Arceneaux, C
Areeda, J
Aston, SM
Astone, P
Aufmuth, P
Aulbert, C
Austin, L
Aylott, BE
Babak, S
Baker, PT
Ballardin, G
Ballmer, SW
Barayoga, JC
Barbet, M
Barish, BC
Barker, D
Barone, F
Barr, B
Barsotti, L
Barsuglia, M
Barton, MA
Bartos, I
Bassiri, R
Basti, A
Batch, JC
Bauchrowitz, J
Bauer, TS
Behnke, B
Bejger, M
Beker, MG
Belczynski, C
Bell, AS
Bell, C
Bergmann, G
Bersanetti, D
Bertolini, A
Betzwieser, J
Beyersdorf, PT
Bilenko, IA
Billingsley, G
Birch, J
Biscans, S
Bitossi, M
Bizouard, MA
Black, E
Blackburn, JK
Blackburn, L
Blair, D
Bloemen, S
Blom, M
Bock, O
Bodiya, TP
Boer, M
Bogaert, G
Bogan, C
Bond, C
Bondu, F
Bonelli, L
Bonnand, R
Bork, R
Born, M
Borkowski, K
Boschi, V
Bose, S
Bosi, L
Bradaschia, C
Brady, PR
Braginsky, VB
Branchesi, M
Brau, JE
Briant, T
Bridges, DO
Brillet, A
Brinkmann, M
Brisson, V
Brooks, AF
Brown, DA
Brown, DD
Bruckner, F
Buchman, S
Bulik, T
Bulten, HJ
Buonanno, A
Burman, R
Buskulic, D
Buy, C
Cadonati, L
Cagnoli, G
Bustillo, JC
Calloni, E
Camp, JB
Campsie, P
Cannon, KC
Canuel, B
Cao, J
Capano, CD
Carbognani, F
Carbone, L
Caride, S
Castiglia, A
Caudill, S
Cavalier, F
Cavalieri, R
Celerier, C
Cella, G
Cepeda, C
Cesarini, E
Chakraborty, R
Chalermsongsak, T
Chamberlin, SJ
Chao, S
Charlton, P
Mottin, EC
Chen, X
Chen, Y
Chincarini, A
Chiummo, A
Cho, HS
Chow, J
Christensen, N
Chu, Q
Chua, SSY
Chung, S
Ciani, G
Clara, F
Clark, JA
Cleva, F
Coccia, E
Cohadon, PF
Colla, A
Collette, C
Colombini, M
Cominsky, L
Conte, A
Cook, D
Corbitt, TR
Cordier, M
Cornish, N
Corpuz, A
Corsi, A
Costa, CA
Coughlin, MW
Coughlin, S
Coulon, JP
Countryman, S
Couvares, P
Coward, DM
Cowart, M
Coyne, DC
Coyne, R
Craig, K
Creighton, JDE
Crowder, SG
Cumming, A
Cunningham, L
Cuoco, E
Dahl, K
Dal Canton, T
Damjanic, M
Danilishin, SL
D'Antonio, S
Danzmann, K
Dattilo, V
Daveloza, H
Davier, M
Davies, GS
Daw, EJ
Day, R
Dayanga, T
Debreczeni, G
Degallaix, J
Deleglise, S
Del Pozzo, W
Denker, T
Dent, T
Dereli, H
Dergachev, V
De Rosa, R
DeRosa, RT
DeSalvo, R
Dhurandhar, S
Diaz, M
Di Fiore, L
Di Lieto, A
Di Palma, I
Di Virgilio, A
Donath, A
Donovan, F
Dooley, KL
Doravari, S
Dorosh, O
Dossa, S
Douglas, R
Downes, TP
Drago, M
Drever, RWP
Driggers, JC
Du, Z
Dwyer, S
Eberle, T
Edo, T
Edwards, M
Effler, A
Eggenstein, H
Ehrens, P
Eichholz, J
Eikenberry, SS
Endroczi, G
Essick, R
Etzel, T
Evans, M
Evans, T
Factourovich, M
Fafone, V
Fairhurst, S
Fang, Q
Farinon, S
Farr, B
Farr, WM
Favata, M
Fehrmann, H
Fejer, MM
Feldbaum, D
Feroz, F
Ferrante, I
Ferrini, F
Fidecaro, F
Finn, LS
Fiori, I
Fisher, RP
Flaminio, R
Fournier, JD
Franco, S
Frasca, S
Frasconi, F
Frede, M
Frei, Z
Freise, A
Frey, R
Fricke, TT
Fritschel, P
Frolov, VV
Fulda, P
Fyffe, M
Gair, J
Gammaitoni, L
Gaonkar, S
Garufi, F
Gehrels, N
Gemme, G
Genin, E
Gennai, A
Ghosh, S
Giaime, JA
Giardina, KD
Giazotto, A
Gill, C
Gleason, J
Goetz, E
Goetz, R
Gondan, L
Gonzalez, G
Gordon, N
Gorodetsky, ML
Gossan, S
Gossler, S
Gouaty, R
Graf, C
Graff, PB
Granata, M
Grant, A
Gras, S
Gray, C
Greenhalgh, RJS
Gretarsson, AM
Groot, P
Grote, H
Grover, K
Grunewald, S
Guidi, GM
Guido, C
Gushwa, K
Gustafson, EK
Gustafson, R
Hammer, D
Hammond, G
Hanke, M
Hanks, J
Hanna, C
Hanson, J
Harms, J
Harry, GM
Harry, IW
Harstad, ED
Hart, M
Hartman, MT
Haster, CJ
Haughian, K
Heidmann, A
Heintze, M
Heitmann, H
Hello, P
Hemming, G
Hendry, M
Heng, IS
Heptonstall, AW
Heurs, M
Hewitson, M
Hild, S
Hoak, D
Hodge, KA
Holt, K
Hooper, S
Hopkins, P
Hosken, DJ
Hough, J
Howell, EJ
Hu, Y
Huerta, E
Hughey, B
Husa, S
Huttner, SH
Huynh, M
Dinh, TH
Ingram, DR
Inta, R
Isogai, T
Ivanov, A
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TI Implementation of an F-statistic all-sky search for continuous
gravitational waves in Virgo VSR1 data
SO CLASSICAL AND QUANTUM GRAVITY
LA English
DT Article
DE gravitational waves; gravitational radiation detectors; pulsars; data
analysis: algorithms and implementation
ID RADIATION
AB We present an implementation of the F-statistic to carry out the first search in data from the Virgo laser interferometric gravitational wave detector for periodic gravitational waves from a priori unknown, isolated rotating neutron stars. We searched a frequency f(0) range from 100 Hz to 1 kHz and the frequency dependent spindown f(1) range from -1.6(f(0)/100 Hz) x 10(-9) Hz s(-1) to zero. A large part of this frequency-spindown space was unexplored by any of the all-sky searches published so far. Our method consisted of a coherent search over two-day periods using the F-statistic, followed by a search for coincidences among the candidates from the two-day segments. We have introduced a number of novel techniques and algorithms that allow the use of the fast Fourier transform (FFT) algorithm in the coherent part of the search resulting in a fifty-fold speed-up in computation of the F-statistic with respect to the algorithm used in the other pipelines. No significant gravitational wave signal was found. The sensitivity of the search was estimated by injecting signals into the data. In the most sensitive parts of the detector band more than 90% of signals would have been detected with dimensionless gravitational-wave amplitude greater than 5 x 10(-24).
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[Cho, H. S.; Kim, Y. M.; Lee, C. H.] Pusan Natl Univ, Pusan 609735, South Korea.
[Chow, J.; Chua, S. S. Y.; McClelland, D. E.; Nguyen, T.; Scott, S. M.; Shaddock, D.; Slagmolen, B. J. J.; Wade, A.; Ward, R. L.] Australian Natl Univ, Canberra, ACT 0200, Australia.
[Christensen, N.; Dossa, S.] Carleton Coll, Northfield, MN 55057 USA.
[Coccia, E.] Ist Nazl Fis Nucl, Gran Sasso Sci Inst, I-67100 Laquila, Italy.
[Coccia, E.; Fafone, V.; Lorenzini, M.; Malvezzi, V.; Nardecchia, I.; Re, V.; Sequino, V.; Sperandio, L.] Univ Roma Tor Vergata, I-00133 Rome, Italy.
[Colla, A.; Conte, A.; Frasca, S.; Mangano, V.; Naticchioni, L.; Rapagnani, P.; Ricci, F.] Univ Roma La Sapienza, I-00185 Rome, Italy.
[Collette, C.] Univ Brussels, B-1050 Brussels, Belgium.
[Cominsky, L.; McLin, K.] Sonoma State Univ, Rohnert Pk, CA 94928 USA.
[Corpuz, A.; Gretarsson, A. M.; Hughey, B.; Loew, K.; Rhoades, E.; Zanolin, M.] Embry Riddle Aeronaut Univ, Prescott, AZ 86301 USA.
[Corsi, A.; Coyne, R.] George Washington Univ, Washington, DC 20052 USA.
[Coughlin, M. W.; Feroz, F.; Gair, J.] Univ Cambridge, Cambridge CB2 1TN, England.
[Coughlin, S.; Farr, B.; Kalogera, V.; Larson, S.; Littenberg, T. B.; Luijten, E.; Scheuer, J.; Shahriar, M. S.; Yablon, J.] Northwestern Univ, Evanston, IL 60208 USA.
[Crowder, S. G.; Kremin, A.; Mandic, V.; Meyers, P.; Prestegard, T.] Univ Minnesota, Minneapolis, MN 55455 USA.
[Daveloza, H.; Diaz, M.; Morriss, S. R.; Mukherjee, S.; Normandin, M. E. N.; Puncken, O.; Quetschke, V.; Rakhmanov, M.; Ramirez, K.; Stone, R.; Torres, C. V.; Valdes, G.] Univ Texas Brownsville, Brownsville, TX 78520 USA.
[Daw, E. J.; Edo, T.; Tomlinson, C.; White, D. J.] Univ Sheffield, Sheffield S10 2TN, S Yorkshire, England.
[Debreczeni, G.; Endroczi, G.; Nagy, M. F.; Racz, I.; Vasuth, M.] Wigner RCP, RMKI, H-1121 Budapest, Hungary.
[DeSalvo, R.; Pierro, V.; Pinto, I. M.] Univ Sannio Benevento, I-82100 Benevento, Italy.
[Dorosh, O.; Krolak, A.; Kutynia, A.; Zadrozny, A.] NCBJ, PL-05400 Otwock, Poland.
[Drago, M.; Leonardi, M.; Prodi, G. A.] Ist Nazl Fis Nucl, Grp Collegato Trento, I-38050 Povo, Trento, Italy.
[Drago, M.; Leonardi, M.; Prodi, G. A.] Univ Trento, I-38050 Povo, Trento, Italy.
[Favata, M.] Montclair State Univ, Montclair, NJ 07043 USA.
[Finn, L. S.; Inta, R.; Owen, B. J.] Penn State Univ, University Pk, PA 16802 USA.
[Frei, Z.; Gondan, L.; Raffai, P.] MTA Eotvos Univ, Lendulet ARG, H-1117 Budapest, Hungary.
[Gammaitoni, L.; Neri, I.; Travasso, F.; Vocca, H.] Univ Perugia, I-06123 Perugia, Italy.
[Greenhalgh, R. J. S.; O'Dell, J.] Rutherford Appleton Lab, HSIC, Didcot OX11 0QX, Oxon, England.
[Hanna, C.] Perimeter Inst Theoret Phys, Waterloo, ON N2L 2Y5, Canada.
[Harry, G. M.] Amer Univ, Washington, DC 20016 USA.
[Hosken, D. J.; King, E. J.; Munch, J.; Ottaway, D. J.; Veitch, P. J.] Univ Adelaide, Adelaide, SA 5005, Australia.
[Iyer, B. R.] Raman Res Inst, Bangalore 560080, Karnataka, India.
[Jang, H.; Kang, G.; Kim, C.; Kim, N. G.] Korea Inst Sci & Technol Informat, Taejon 305806, South Korea.
[Jaranowski, P.] Bialystok Univ, PL-15424 Bialystok, Poland.
[Jones, D. I.] Univ Southampton, Southampton SO17 1BJ, Hants, England.
[Haris, K.; Mazumder, N.; Mishra, C.; Pai, A.] IISER TVM, Trivandrum 695016, Kerala, India.
[Khazanov, E. A.; Palashov, O.; Poteomkin, A.; Sergeev, A.] Inst Appl Phys, Nizhnii Novgorod 603950, Russia.
[Kim, C.; Lee, H. M.] Seoul Natl Univ, Seoul 151742, South Korea.
[Kim, K.; Lee, H. K.] Hanyang Univ, Seoul 133791, South Korea.
[Krolak, A.] IM PAN, PL-00956 Warsaw, Poland.
[Kumar, A.] Inst Plasma Res, Bhat 382428, Gandhinagar, India.
[Lasky, P. D.; Melatos, A.; Sammut, L.] Univ Melbourne, Parkville, Vic 3010, Australia.
[Lazzaro, C.; Vedovato, G.; Zendri, J. P.] Ist Nazl Fis Nucl, Sez Padova, I-35131 Padua, Italy.
[Levin, Y.; Premachandra, S.] Monash Univ, Clayton, Vic 3800, Australia.
[Lockerbie, N. A.; Tokmakov, K. V.] Univ Strathclyde, SUPA, Glasgow G1 1XQ, Lanark, Scotland.
[Loriette, V.; Maksimovic, I.] CNRS, ESPCI, F-75005 Paris, France.
[Maglione, C.; Quiroga, G.] Argentinian Gravitat Wave Grp, RA-5000 Cordoba Cordoba, Argentina.
[Marchesoni, F.] Univ Camerino, Dipartimento Fis, I-62032 Camerino, Italy.
[Matzner, R. A.] Univ Texas Austin, Austin, TX 78712 USA.
[McGuire, S. C.; Finley, R. Vincent; Williams, K.] Southern Univ, Baton Rouge, LA 70813 USA.
[McGuire, S. C.; Finley, R. Vincent; Williams, K.] A&M Coll, Baton Rouge, LA 70813 USA.
[Mikhailov, E. E.; Romanov, G.] Coll William & Mary, Williamsburg, VA 23187 USA.
[Nayak, R. K.] IISER Kolkata, Mohanpur 741252, W Bengal, India.
[Oh, J. J.; Oh, S. H.; Son, E. J.] Natl Inst Math Sci, Taejon 305390, South Korea.
[Penn, S.] Hobart & William Smith Coll, Geneva, NY 14456 USA.
[Pietka, M.] Gjovik Videregaende Skole, N-2803 Gjovik, Norway.
[Raja, S.] RRCAT, Indore 452013, Madhya Pradesh, India.
[Reid, S.] Univ West Scotland, SUPA, Paisley PA1 2BE, Renfrew, Scotland.
[Rosinska, D.] Inst Astron, PL-65265 Zielona Gora, Poland.
[Sengupta, A. S.] Indian Inst Technol, Ahmadabad 382424, Gujarat, India.
[Sturani, R.] Univ Estadual Paulista, Int Theoret Phys, South Amer Inst Res, Inst Fis Teor, BR-01140070 Sao Paulo, Brazil.
[Summerscales, T. Z.] Andrews Univ, Berrien Springs, MI 49104 USA.
[Ugolini, D.] Trinity Univ, San Antonio, TX 78212 USA.
[Venkateswara, K.] Univ Washington, Seattle, WA 98195 USA.
[Williams, T.; Yoshida, S.] SE Louisiana Univ, Hammond, LA 70402 USA.
[Willis, J. L.] Abilene Christian Univ, Abilene, TX 79699 USA.
RP Aasi, J (reprint author), CALTECH, LIGO, Pasadena, CA 91125 USA.
RI Aggarwal, Nancy/M-7203-2015; Shaddock, Daniel/A-7534-2011; Vicere,
Andrea/J-1742-2012; Rocchi, Alessio/O-9499-2015; Martelli,
Filippo/P-4041-2015; Branchesi, Marica/P-2296-2015; Gehring,
Tobias/A-8596-2016; Strain, Kenneth/D-5236-2011; Howell,
Eric/H-5072-2014; Heidmann, Antoine/G-4295-2016; Nelemans,
Gijs/D-3177-2012; Marchesoni, Fabio/A-1920-2008; Zhu,
Xingjiang/E-1501-2016; M, Manjunath/N-4000-2014; Vecchio,
Alberto/F-8310-2015; Strigin, Sergey/I-8337-2012; Leonardi,
Matteo/G-9694-2015; Sigg, Daniel/I-4308-2015; Puppo, Paola/J-4250-2012;
Tacca, Matteo/J-1599-2015; Graef, Christian/J-3167-2015; Bell,
Angus/E-7312-2011; Ottaway, David/J-5908-2015; Garufi,
Fabio/K-3263-2015; Deleglise, Samuel/B-1599-2015; Neri,
Igor/F-1482-2010; Steinlechner, Sebastian/D-5781-2013; Khalili,
Farit/D-8113-2012; Gorodetsky, Michael/C-5938-2008; McClelland,
David/E-6765-2010; Hild, Stefan/A-3864-2010; Gammaitoni,
Luca/B-5375-2009; Gemme, Gianluca/C-7233-2008; Iyer, Bala
R./E-2894-2012; prodi, giovanni/B-4398-2010; Canuel,
Benjamin/C-7459-2014; Danilishin, Stefan/K-7262-2012; Prokhorov,
Leonid/I-2953-2012; Lee, Chang-Hwan/B-3096-2015; Frasconi,
Franco/K-1068-2016; Groot, Paul/K-4391-2016; Lazzaro,
Claudia/L-2986-2016; Pinto, Innocenzo/L-3520-2016; Ferrante,
Isidoro/F-1017-2012; Losurdo, Giovanni/K-1241-2014; Travasso,
Flavio/J-9595-2016; Bartos, Imre/A-2592-2017; Punturo,
Michele/I-3995-2012; Cella, Giancarlo/A-9946-2012; Cesarini,
Elisabetta/C-4507-2017; Costa, Cesar/G-7588-2012; Chow,
Jong/A-3183-2008; Frey, Raymond/E-2830-2016; Ciani, Giacomo/G-1036-2011;
Di Virgilio, Angela Dora Vittoria/E-9078-2015; Sergeev,
Alexander/F-3027-2017; Harms, Jan/J-4359-2012; Ward, Robert/I-8032-2014;
OI Shaddock, Daniel/0000-0002-6885-3494; Vicere,
Andrea/0000-0003-0624-6231; Rocchi, Alessio/0000-0002-1382-9016;
Martelli, Filippo/0000-0003-3761-8616; Gehring,
Tobias/0000-0002-4311-2593; Strain, Kenneth/0000-0002-2066-5355; Howell,
Eric/0000-0001-7891-2817; Heidmann, Antoine/0000-0002-0784-5175;
Nelemans, Gijs/0000-0002-0752-2974; Marchesoni,
Fabio/0000-0001-9240-6793; Zhu, Xingjiang/0000-0001-7049-6468; M,
Manjunath/0000-0001-8710-0730; Vecchio, Alberto/0000-0002-6254-1617;
Sigg, Daniel/0000-0003-4606-6526; Puppo, Paola/0000-0003-4677-5015;
Tacca, Matteo/0000-0003-1353-0441; Graef, Christian/0000-0002-4535-2603;
Bell, Angus/0000-0003-1523-0821; Garufi, Fabio/0000-0003-1391-6168;
Deleglise, Samuel/0000-0002-8680-5170; Neri, Igor/0000-0002-9047-9822;
Steinlechner, Sebastian/0000-0003-4710-8548; Gorodetsky,
Michael/0000-0002-5159-2742; McClelland, David/0000-0001-6210-5842;
Gammaitoni, Luca/0000-0002-4972-7062; Gemme,
Gianluca/0000-0002-1127-7406; Iyer, Bala R./0000-0002-4141-5179; prodi,
giovanni/0000-0001-5256-915X; Danilishin, Stefan/0000-0001-7758-7493;
Lee, Chang-Hwan/0000-0003-3221-1171; Frasconi,
Franco/0000-0003-4204-6587; Groot, Paul/0000-0002-4488-726X; Lazzaro,
Claudia/0000-0001-5993-3372; Ferrante, Isidoro/0000-0002-0083-7228;
Losurdo, Giovanni/0000-0003-0452-746X; Travasso,
Flavio/0000-0002-4653-6156; Punturo, Michele/0000-0001-8722-4485; Cella,
Giancarlo/0000-0002-0752-0338; Cesarini, Elisabetta/0000-0001-9127-3167;
Chow, Jong/0000-0002-2414-5402; Frey, Raymond/0000-0003-0341-2636;
Ciani, Giacomo/0000-0003-4258-9338; Di Virgilio, Angela Dora
Vittoria/0000-0002-2237-7533; Ward, Robert/0000-0001-5503-5241; Whelan,
John/0000-0001-5710-6576; Vedovato, Gabriele/0000-0001-7226-1320;
Fairhurst, Stephen/0000-0001-8480-1961; Matichard,
Fabrice/0000-0001-8982-8418; Husa, Sascha/0000-0002-0445-1971; Vocca,
Helios/0000-0002-1200-3917; Farr, Ben/0000-0002-2916-9200; Collette,
Christophe/0000-0002-4430-3703; Coccia, Eugenio/0000-0002-6669-5787;
Vetrano, Flavio/0000-0002-7523-4296; Addesso, Paolo/0000-0003-0895-184X;
Naticchioni, Luca/0000-0003-2918-0730; calloni,
enrico/0000-0003-4819-3297; Bondu, Francois/0000-0001-6487-5197;
Zweizig, John/0000-0002-1521-3397; Del Pozzo,
Walter/0000-0003-3978-2030; O'Shaughnessy, Richard/0000-0001-5832-8517;
Granata, Massimo/0000-0003-3275-1186; Kanner, Jonah/0000-0001-8115-0577;
Freise, Andreas/0000-0001-6586-9901; Mandel, Ilya/0000-0002-6134-8946;
Whiting, Bernard F/0000-0002-8501-8669; Ricci,
Fulvio/0000-0001-5475-4447; Boschi, Valerio/0000-0001-8665-2293; Pinto,
Innocenzo M./0000-0002-2679-4457; Guidi, Gianluca/0000-0002-3061-9870;
Pierro, Vincenzo/0000-0002-6020-5521; Scott, Jamie/0000-0001-6701-6515;
Sorazu, Borja/0000-0002-6178-3198
FU United States National Science Foundation; Science and Technology
Facilities Council of the United Kingdom; Max-Planck-Society; State of
Niedersachsen/Germany; Australian Research Council; International
Science Linkages program of the Commonwealth of Australia; Council of
Scientific and Industrial Research of India; Istituto Nazionale di
Fisica Nucleare of Italy; Spanish Ministerio de Economia y
Competitividad; Conselleria d'Economia Hisenda i Innovacio of the Govern
de les Illes Balears; Foundation for Fundamental Research; Netherlands
Organisation; Polish Ministry of Science and Higher Education; FOCUS
Programme of Foundation for Polish Science; PL-Grid Infrastructure;
Royal Society; Scottish Funding Council; Scottish Universities Physics
Alliance; National Aeronautics and Space Administration; Carnegie Trust;
Leverhulme Trust; David and Lucile Packard Foundation; Research
Corporation; Alfred P Sloan Foundation
FX The authors gratefully acknowledge the support of the United States
National Science Foundation for the construction and operation of the
LIGO Laboratory, the Science and Technology Facilities Council of the
United Kingdom, the Max-Planck-Society and the State of
Niedersachsen/Germany for support of the construction and operation of
the GEO600 detector, and the Italian Istituto Nazionale di Fisica
Nucleare and the French Centre National de la Recherche Scientifique for
the construction and operation of the Virgo detector. The authors also
gratefully acknowledge the support of the research by these agencies and
by the Australian Research Council, the International Science Linkages
program of the Commonwealth of Australia, the Council of Scientific and
Industrial Research of India, the Istituto Nazionale di Fisica Nucleare
of Italy, the Spanish Ministerio de Economia y Competitividad, the
Conselleria d'Economia Hisenda i Innovacio of the Govern de les Illes
Balears, the Foundation for Fundamental Research on Matter supported by
the Netherlands Organisation for Scientific Research, the Polish
Ministry of Science and Higher Education, the FOCUS Programme of
Foundation for Polish Science, the PL-Grid Infrastructure, the Royal
Society, the Scottish Funding Council, the Scottish Universities Physics
Alliance, The National Aeronautics and Space Administration, the
Carnegie Trust, the Leverhulme Trust, the David and Lucile Packard
Foundation, the Research Corporation, and the Alfred P Sloan Foundation.
This document has been assigned LIGO Laboratory document number
LIGO-P1300133.
NR 23
TC 11
Z9 11
U1 4
U2 47
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0264-9381
EI 1361-6382
J9 CLASSICAL QUANT GRAV
JI Class. Quantum Gravity
PD AUG 21
PY 2014
VL 31
IS 16
AR 165014
DI 10.1088/0264-9381/31/16/165014
PG 27
WC Astronomy & Astrophysics; Physics, Multidisciplinary; Physics, Particles
& Fields
SC Astronomy & Astrophysics; Physics
GA AO5XX
UT WOS:000341421600014
ER
PT J
AU Steffen, W
Teodoro, M
Madura, TI
Groh, JH
Gull, TR
Mehner, A
Corcoran, MF
Damineli, A
Hamaguchi, K
AF Steffen, W.
Teodoro, M.
Madura, T. I.
Groh, J. H.
Gull, T. R.
Mehner, A.
Corcoran, M. F.
Damineli, A.
Hamaguchi, K.
TI The three-dimensional structure of the Eta Carinae Homunculus
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE methods: numerical; circumstellar matter; stars: individual: Eta
Carinae; stars: mass-loss; stars: winds; outflows
ID HUBBLE-SPACE-TELESCOPE; LUMINOUS BLUE VARIABLES; PLANETARY-NEBULAE;
COLLIDING WINDS; STELLAR WINDS; MASS-LOSS; INFRARED MORPHOLOGY;
PERIASTRON PASSAGE; EDDINGTON LIMIT; LIGHT-CURVE
AB We investigate, using the modelling code shape, the three-dimensional structure of the bipolar Homunculus nebula surrounding Eta Carinae as mapped by new ESO Very Large Telescope/X-Shooter observations of the H-2 lambda = 2.121 25 mu m emission line. Our results reveal for the first time important deviations from the axisymmetric bipolar morphology: (1) circumpolar trenches in each lobe positioned point symmetrically from the centre and (2) off-planar protrusions in the equatorial region from each lobe at longitudinal (similar to 55A degrees) and latitudinal (10A degrees-20A degrees) distances from the projected apastron direction of the binary orbit. The angular distance between the protrusions (similar to 110A degrees) is similar to the angular extent of each polar trench (similar to 130A degrees) and nearly equal to the opening angle of the wind-wind collision cavity (similar to 110A degrees). As in previous studies, we confirm a hole near the centre of each polar lobe and no detectable near-IR H-2 emission from the thin optical skirt seen prominently in visible imagery. We conclude that the interaction between the outflows and/or radiation from the central binary stars and their orientation in space has had, and possibly still has, a strong influence on the Homunculus. This implies that prevailing theoretical models of the Homunculus are incomplete as most assume a single-star origin that produces an axisymmetric nebula. We discuss how the newly found features might be related to the Homunculus ejection, the central binary, and the interacting stellar winds.
C1 [Steffen, W.] Univ Nacl Autonoma Mexico, Inst Astron, Ensenada 22800, Baja California, Mexico.
[Teodoro, M.; Madura, T. I.; Gull, T. R.] NASA, Astrophys Sci Div, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Groh, J. H.] Univ Geneva, Observ Geneva, CH-1290 Sauverny, Switzerland.
[Mehner, A.] ESO, Vitacura, Santiago De Chi, Chile.
[Corcoran, M. F.; Hamaguchi, K.] NASA, CRESST, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Corcoran, M. F.; Hamaguchi, K.] NASA, Xray Astrophys Lab, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Corcoran, M. F.] Univ Space Res Assoc, Columbia, MD 21046 USA.
[Damineli, A.] Univ Sao Paulo, Inst Astron Geofis & Ciencias Atmosfer, BR-05508900 Sao Paulo, Brazil.
[Hamaguchi, K.] Univ Maryland Baltimore Cty, Dept Phys, Baltimore, MD 21250 USA.
RP Steffen, W (reprint author), Univ Nacl Autonoma Mexico, Inst Astron, Apdo Postal 106, Ensenada 22800, Baja California, Mexico.
EM wsteffen@astro.unam.mx
RI Damineli, Augusto/P-8829-2016
OI Damineli, Augusto/0000-0002-7978-2994
FU UNAM-PAPIIT [IN101014]; CNPq/MCT-Brazil [201978/2012-1]; NASA
Postdoctoral Program at the Goddard Space Flight Center; Swiss National
Science Foundation; FAPESP
FX WS acknowledges financial support through grant UNAM-PAPIIT IN101014. MT
is supported by CNPq/MCT-Brazil through grant 201978/2012-1. TIM is
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. JHG is supported by an
Ambizione fellowship of the Swiss National Science Foundation. AD
acknowledges FAPESP for continuous financial support. The authors thank
D. Clark for useful discussions.
NR 96
TC 9
Z9 9
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 AUG 21
PY 2014
VL 442
IS 4
BP 3316
EP 3328
DI 10.1093/mnras/stu1088
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AM5TZ
UT WOS:000339924900042
ER
PT J
AU Buckley, MR
Zavala, J
Cyr-Racine, FY
Sigurdson, K
Vogelsberger, M
AF Buckley, Matthew R.
Zavala, Jesus
Cyr-Racine, Francis-Yan
Sigurdson, Kris
Vogelsberger, Mark
TI Scattering, damping, and acoustic oscillations: Simulating the structure
of dark matter halos with relativistic force carriers
SO PHYSICAL REVIEW D
LA English
DT Article
ID DWARF SPHEROIDAL GALAXIES; LARGE-SCALE STRUCTURE; LYMAN-ALPHA FOREST;
POWER SPECTRUM; LAMBDA-CDM; MILLICHARGED PARTICLES; BARYONS MATTER; MASS
FUNCTION; MIRROR WORLD; SUBSTRUCTURE
AB We demonstrate that self-interacting dark matter models with interactions mediated by light particles can have significant deviations in the matter power spectrum and detailed structure of galactic halos when compared to a standard cold dark matter scenario. While these deviations can take the form of suppression of small-scale structure that are in some ways similar to that of warm dark matter, the self-interacting models have a much wider range of possible phenomenology. A long-range force in the dark matter can introduce multiple scales to the initial power spectrum, in the form of dark acoustic oscillations and an exponential cutoff in the power spectrum. Using simulations we show that the impact of these scales can remain observationally relevant up to the present day. Furthermore, the self-interaction can continue to modify the small-scale structure of the dark matter halos, reducing their central densities and creating a dark matter core. The resulting phenomenology is unique to these type of models.
C1 [Buckley, Matthew R.] Rutgers State Univ, Dept Phys & Astron, Piscataway, NJ 08854 USA.
[Zavala, Jesus] Univ Copenhagen, Niels Bohr Inst, Dark Cosmol Ctr, DK-2100 Copenhagen, Denmark.
[Cyr-Racine, Francis-Yan] CALTECH, Jet Prop Lab, NASA, Pasadena, CA 91109 USA.
[Cyr-Racine, Francis-Yan] CALTECH, Pasadena, CA 91125 USA.
[Sigurdson, Kris] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada.
[Vogelsberger, Mark] MIT, Dept Phys, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA.
RP Buckley, MR (reprint author), Rutgers State Univ, Dept Phys & Astron, POB 849, Piscataway, NJ 08854 USA.
OI Buckley, Matthew/0000-0003-1109-3460; Cyr-Racine,
Francis-Yan/0000-0002-7939-2988
FU National Science Foundation [1066293]; W. M. Keck Foundation; National
Aeronautics and Space Administration; National Science and Engineering
Research Council (NSERC) of Canada Discovery Grant; DNRF; EU under a
Marie Curie International Incoming Fellowship [PIIF-GA-2013-627723]
FX M. R. B. would like to thank Alyson Brooks for useful discussion and
comments. M. R. B. and J. Z. thank the Aspen Center for Physics, where
the initial conversations that led to their interest in this project
were held. The Aspen Center for Physics is supported by the National
Science Foundation under Grant No. 1066293. The work of F. Y. C. R. was
performed in part at the California Institute of Technology for the Keck
Institute for Space Studies, which is funded by the W. M. Keck
Foundation. Part of 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.
The research of K. S. is supported in part by a National Science and
Engineering Research Council (NSERC) of Canada Discovery Grant. The Dark
Cosmology Centre is funded by the DNRF. J. Z. is supported by the EU
under a Marie Curie International Incoming Fellowship, Contract No.
PIIF-GA-2013-627723. The simulations in this paper were carried out on
the Gardar supercomputer supported by the Nordic High Performance
Computing (NHPC).
NR 158
TC 36
Z9 36
U1 0
U2 2
PU AMER PHYSICAL SOC
PI COLLEGE PK
PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA
SN 2470-0010
EI 2470-0029
J9 PHYS REV D
JI Phys. Rev. D
PD AUG 20
PY 2014
VL 90
IS 4
AR 043524
DI 10.1103/PhysRevD.90.043524
PG 21
WC Astronomy & Astrophysics; Physics, Particles & Fields
SC Astronomy & Astrophysics; Physics
GA AT2SH
UT WOS:000344785100005
ER
PT J
AU Latvakoski, H
Mlynczak, MG
Cageao, RP
Johnson, DG
Kratz, DP
AF Latvakoski, Harri
Mlynczak, Martin G.
Cageao, Richard P.
Johnson, David G.
Kratz, David P.
TI Far-infrared spectroscopy of the troposphere: calibration with a cold
background
SO APPLIED OPTICS
LA English
DT Article
ID PERFORMANCE; INSTRUMENT
AB The far-infrared spectroscopy of the troposphere (FIRST) instrument is a Fourier-transform spectrometer developed to measure the Earth's thermal emission spectrum with a particular emphasis on the far-infrared. FIRST has observed the atmosphere from both the ground looking up and from a high-altitude balloon looking down. A recent absolute laboratory calibration of FIRST under ground-like operating conditions showed accuracy to better than 0.3 K at near-ambient temperatures (270-325 K) but reduced accuracy at lower temperatures. This paper presents calibration results for balloon-flight conditions using a cold blackbody to simulate the space view used for on-board calibration. An unusual detector nonlinearity was discovered and corrected, and stray light was measured and removed. Over most of the range of Earth scene temperatures (205-300 K), the accuracy of FIRST is 0.35-0.15 K (one sigma). (C) 2014 Optical Society of America
C1 [Latvakoski, Harri] Space Dynam Lab, North Logan, UT 84341 USA.
[Mlynczak, Martin G.; Kratz, David P.] NASA, Langley Res Ctr, Sci Directorate, Hampton, VA 23681 USA.
[Cageao, Richard P.; Johnson, David G.] NASA, Langley Res Ctr, Engn Directorate, Hampton, VA 23681 USA.
RP Mlynczak, MG (reprint author), NASA, Langley Res Ctr, Sci Directorate, Mail Stop 420, Hampton, VA 23681 USA.
EM m.g.mlynczak@nasa.gov
RI Johnson, David/F-2376-2015; Richards, Amber/K-8203-2015
OI Johnson, David/0000-0003-4399-5653;
NR 13
TC 1
Z9 1
U1 0
U2 5
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 AUG 20
PY 2014
VL 53
IS 24
BP 5425
EP 5433
DI 10.1364/AO.53.005425
PG 9
WC Optics
SC Optics
GA AN8BE
UT WOS:000340825000026
PM 25321115
ER
PT J
AU Arevalo, P
Bauer, FE
Puccetti, S
Walton, DJ
Koss, M
Boggs, SE
Brandt, WN
Brightman, M
Christensen, FE
Comastri, A
Craig, WW
Fuerst, F
Gandhi, P
Grefenstette, BW
Hailey, CJ
Harrison, FA
Luo, B
Madejski, G
Madsen, KK
Marinucci, A
Matt, G
Saez, C
Stern, D
Stuhlinger, M
Treister, E
Urry, CM
Zhang, WW
AF Arevalo, P.
Bauer, F. E.
Puccetti, S.
Walton, D. J.
Koss, M.
Boggs, S. E.
Brandt, W. N.
Brightman, M.
Christensen, F. E.
Comastri, A.
Craig, W. W.
Fuerst, F.
Gandhi, P.
Grefenstette, B. W.
Hailey, C. J.
Harrison, F. A.
Luo, B.
Madejski, G.
Madsen, K. K.
Marinucci, A.
Matt, G.
Saez, C.
Stern, D.
Stuhlinger, M.
Treister, E.
Urry, C. M.
Zhang, W. W.
TI THE 2-79 keV X-RAY SPECTRUM OF THE CIRCINUS GALAXY WITH NuSTAR,
XMM-Newton, AND CHANDRA: A FULLY COMPTON-THICK ACTIVE GALACTIC NUCLEUS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: active; galaxies: individual (Circinus); galaxies: Seyfert;
X-rays: galaxies
ID STAR-FORMATION RATE; SEYFERT-GALAXIES; NEARBY SEYFERT; RATE INDICATOR;
LINE REGION; BEPPOSAX; VIEW; SPECTROSCOPY; ACCRETION; AGN
AB The Circinus galaxy is one of the closest obscured active galactic nuclei (AGNs), making it an ideal target for detailed study. Combining archival Chandra and XMM-Newton data with new NuSTAR observations, we model the 2-79 keV spectrum to constrain the primary AGN continuum and to derive physical parameters for the obscuring material. Chandra's high angular resolution allows a separation of nuclear and off-nuclear galactic emission. In the off-nuclear diffuse emission, we find signatures of strong cold reflection, including high equivalent-width neutral Fe lines. This Compton-scattered off-nuclear emission amounts to 18% of the nuclear flux in the Fe line region, but becomes comparable to the nuclear emission above 30 keV. The new analysis no longer supports a prominent transmitted AGN component in the observed band. We find that the nuclear spectrum is consistent with Compton scattering by an optically thick torus, where the intrinsic spectrum is a power law of photon index Gamma = 2.2-2.4, the torus has an equatorial column density of N-H = (6-10) x 10(24) cm(-2), and the intrinsic AGN 2-10 keV luminosity is (2.3-5.1) x10(42) erg s(-1). These values place Circinus along the same relations as unobscured AGNs in accretion rate versus Gamma and L-X versus L-IR phase space. NuSTAR's high sensitivity and low background allow us to study the short timescale variability of Circinus at X-ray energies above 10 keV for the first time. The lack of detected variability favors a Compton-thick absorber, in line with the spectral fitting results.
C1 [Arevalo, P.; Bauer, F. E.; Saez, C.] Pontificia Univ Catolica Chile, Fac Fis, Inst Astrofis, Santiago 22, Chile.
[Arevalo, P.] Univ Valparaiso, Fac Ciencias, Inst Fis & Astron, Valparaiso, Chile.
[Bauer, F. E.] Millennium Inst Astrophys, Boulder, CO 80301 USA.
[Bauer, F. E.] Space Sci Inst, Boulder, CO 80301 USA.
[Puccetti, S.] ASDC, ASI, I-00133 Rome, Italy.
[Puccetti, S.] Osserv Astron Roma, INAF, I-00040 Monte Porzio Catone, RM, Italy.
[Walton, D. J.; Fuerst, F.; Grefenstette, B. W.; Harrison, F. A.; Madsen, K. K.] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA.
[Koss, M.] ETH, Inst Astron, Dept Phys, CH-8093 Zurich, Switzerland.
[Boggs, S. E.; Craig, W. W.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
[Brandt, W. N.; Luo, B.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA.
[Brandt, W. N.; Luo, B.] Penn State Univ, Inst Gravitat & Cosmos, University Pk, PA 16802 USA.
[Brightman, M.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany.
[Christensen, F. E.] Danish Tech Univ, Lyngby, Denmark.
[Comastri, A.] Osservatorio Astron Bologna, INAF, I-40127 Bologna, Italy.
[Craig, W. W.] Lawrence Livermore Natl Lab, Livermore, CA 94550 USA.
[Gandhi, P.] Univ Durham, Dept Phys, Durham DH1 3LE, England.
[Hailey, C. J.] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA.
[Hailey, C. J.] Columbia Univ, Dept Phys, New York, NY 10027 USA.
[Madejski, G.] Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, SLAC Natl Accelerator Lab, Menlo Pk, CA 94025 USA.
[Marinucci, A.; Matt, G.] Univ Roma Tre, Dipartimento Matemat Fis, I-00146 Rome, Italy.
[Saez, C.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Stern, D.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Stuhlinger, M.] ESAC, E-28691 Madrid, Spain.
[Treister, E.] Univ Concepcion, Dept Astron, Concepcion, Chile.
[Urry, C. M.] Yale Univ, Yale Ctr Astron & Astrophys, Dept Phys, New Haven, CT 06520 USA.
[Zhang, W. W.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Arevalo, P (reprint author), Pontificia Univ Catolica Chile, Fac Fis, Inst Astrofis, Santiago 22, Chile.
RI Boggs, Steven/E-4170-2015; Koss, Michael/B-1585-2015; Brandt,
William/N-2844-2015; Comastri, Andrea/O-9543-2015;
OI Boggs, Steven/0000-0001-9567-4224; Koss, Michael/0000-0002-7998-9581;
Brandt, William/0000-0002-0167-2453; Comastri,
Andrea/0000-0003-3451-9970; Puccetti, Simonetta/0000-0002-2734-7835;
Urry, Meg/0000-0002-0745-9792
FU NASA [NNG08FD60C]; National Aeronautics and Space Administration;
Basal-CATA [PFB-06/2007]; CONICYT-Chile FONDECYT [1140304, 1141218,
1120061, Anillo ACT1101]; ASI-INAF grant [I/037/12/0]; Caltech NuSTAR
subcontract [44A-1092750]; NASA ADP grant [NNX10AC99G]; Swiss National
Science Foundation [PP00P2_138979/1]; STFC [ST/J003697/1]
FX We thank the anonymous referee for a thorough review and many useful
suggestions that improved this paper. This work was supported under NASA
Contract No. NNG08FD60C, and made use of data from the NuSTAR mission, a
project led by the California Institute of Technology, managed by the
Jet Propulsion Laboratory, and funded by the National Aeronautics and
Space Administration. We thank the NuSTAR Operations, Software, and
Calibration teams for support with the execution and analysis of these
observations. This research has made use of the NuSTAR Data Analysis
Software (NuSTARDAS) jointly developed by the ASI Science Data Center
(ASDC, Italy) and the California Institute of Technology (USA). We
acknowledge financial support from Basal-CATA PFB-06/2007 (FEB),
CONICYT-Chile FONDECYT 1140304 (PA), 1141218 (FEB), 1120061 (ET), and
Anillo ACT1101 (PA, FEB, ET). A. C., A. M., and G. M. acknowledge the
ASI-INAF grant I/037/12/0. W.N.B. and B. L. acknowledge support from
Caltech NuSTAR subcontract 44A-1092750 and NASA ADP grant NNX10AC99G. M.
K. gratefully acknowledges support from Swiss National Science
Foundation Grant PP00P2_138979/1. P. G. thanks STFC for support (grant
reference ST/J003697/1).
NR 67
TC 38
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U1 2
U2 13
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 AUG 20
PY 2014
VL 791
IS 2
AR 81
DI 10.1088/0004-637X/791/2/81
PG 21
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AM7EV
UT WOS:000340028400008
ER
PT J
AU Bodenheimer, P
Lissauer, JJ
AF Bodenheimer, Peter
Lissauer, Jack J.
TI ACCRETION AND EVOLUTION OF similar to 2.5 M-circle plus PLANETS WITH
VOLUMINOUS H/He ENVELOPES
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE planets and satellites: formation; planets and satellites: individual
(Kepler-11 f); planets and satellites: physical evolution
ID IN-SITU FORMATION; GIANT PLANETS; SUPER-EARTHS; PROTOPLANETARY
ATMOSPHERES; THERMAL EVOLUTION; KEPLER PLANETS; LOW-MASS; MODELS;
PLANETESIMALS; OPACITIES
AB Formation of planets in the Neptune size range with low-mass, but voluminous, H-2/He gaseous envelopes is modeled by detailed numerical simulations according to the core-nucleated accretion scenario. Formation locations ranging from 0.5 to 4 AU from a star of 1 M-circle dot are considered. The final planets have heavy-element cores of 2.2-2.5 M-circle plus and envelopes in the range 0.037-0.16 M-circle plus. After the formation process, which lasts 2 Myr or less, the planets evolve at constant mass up to an age of several Gyr. For assumed equilibrium temperatures of 250, 500, and 1000 K, their calculated final radii are compared with those observed by the Kepler spacecraft. For the particular case of Kepler-11 f, we address the question whether it could have formed in situ or whether migration from a formation location farther out in the disk is required.
C1 [Bodenheimer, Peter] Univ Calif Santa Cruz, Dept Astron & Astrophys, UCO Lick Observ, Santa Cruz, CA 95064 USA.
[Lissauer, Jack J.] NASA, Ames Res Ctr, Space Sci & Astrobiol Div, Moffett Field, CA 94035 USA.
RP Bodenheimer, P (reprint author), Univ Calif Santa Cruz, Dept Astron & Astrophys, UCO Lick Observ, Santa Cruz, CA 95064 USA.
EM peter@ucolick.org; Jack.J.Lissauer@nasa.gov
OI Bodenheimer, Peter/0000-0001-6093-3097
FU NASA Origins of Solar Systems Program grant [NNX11AK54G]; NSF
[AST0908807]
FX Primary funding for this project was provided by the NASA Origins of
Solar Systems Program grant NNX11AK54G (P.B. and J.L.). P.B.
acknowledges additional support from NSF grant AST0908807.
NR 40
TC 18
Z9 18
U1 0
U2 2
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 AUG 20
PY 2014
VL 791
IS 2
AR 103
DI 10.1088/0004-637X/791/2/103
PG 9
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AM7EV
UT WOS:000340028400030
ER
PT J
AU Bostrom, A
Reynolds, CS
Tombesi, F
AF Bostrom, Allison
Reynolds, Christopher S.
Tombesi, Francesco
TI AN XMM-NEWTON VIEW OF THE RADIO GALAXY 3C 411
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE accretion, accretion disks; black hole physics; galaxies: active;
galaxies: jets; galaxies: individual (3C411); X-rays: galaxies
ID ULTRA-FAST OUTFLOWS; SHELL ABSORPTION-LINES; ACTIVE GALACTIC NUCLEI; BL
LACERTAE OBJECTS; X-RAY; BLACK-HOLE; SEYFERT-GALAXIES; QUIET AGNS;
SPECTRA; BLAZARS
AB We present the first high signal-to-noise XMM-Newton observations of the broad-line radio galaxy 3C 411. After fitting various spectral models, an absorbed double power-law (PL) continuum and a blurred relativistic disk reflection model (kdblur) are found to be equally plausible descriptions of the data. While the softer PL component (Gamma = 2.11) of the double PL model is entirely consistent with that found in Seyfert galaxies (and hence likely originates from a disk corona), the additional PL component is very hard (Gamma = 1.05); amongst the active galactic nucleus zoo, only flat-spectrum radio quasars (FSRQ) have such hard spectra. Together with the flat radio-spectrum displayed by this source, we suggest that it should instead be classified as an FSRQ. This leads to potential discrepancies regarding the jet inclination angle, with the radio morphology suggesting a large jet inclination but the FSRQ classification suggesting small inclinations. The kdblur model predicts an inner disk radius of at most 20 r(g) and relativistic reflection.
C1 [Bostrom, Allison; Reynolds, Christopher S.; Tombesi, Francesco] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Reynolds, Christopher S.] Joint Space Sci Inst JSI, College Pk, MD 20742 USA.
[Reynolds, Christopher S.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Bostrom, A (reprint author), Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
FU NASA [NNX12AE13G]
FX We thank David Ballantyne for interesting and fruitful discussions. C.
S. R. thanks NASA for support under the ADAP program (grant NNX12AE13G).
NR 42
TC 3
Z9 3
U1 0
U2 0
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 AUG 20
PY 2014
VL 791
IS 2
AR 119
DI 10.1088/0004-637X/791/2/119
PG 6
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AM7EV
UT WOS:000340028400046
ER
PT J
AU Dawson, RI
Johnson, JA
Fabrycky, DC
Foreman-Mackey, D
Murray-Clay, RA
Buchhave, LA
Cargile, PA
Clubb, KI
Fulton, BJ
Hebb, L
Howard, AW
Huber, D
Shporer, A
Valenti, JA
AF Dawson, Rebekah I.
Johnson, John Asher
Fabrycky, Daniel C.
Foreman-Mackey, Daniel
Murray-Clay, Ruth A.
Buchhave, Lars A.
Cargile, Phillip A.
Clubb, Kelsey I.
Fulton, Benjamin J.
Hebb, Leslie
Howard, Andrew W.
Huber, Daniel
Shporer, Avi
Valenti, Jeff A.
TI LARGE ECCENTRICITY, LOW MUTUAL INCLINATION: THE THREE-DIMENSIONAL
ARCHITECTURE OF A HIERARCHICAL SYSTEM OF GIANT PLANETS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE planetary systems
ID TRANSIT TIMING VARIATIONS; CANDIDATE HOST STARS; CLOSE-IN PLANETS; HOT
JUPITERS; LIGHT CURVES; DYNAMICAL INSTABILITIES; ORBITAL EVOLUTION;
ERROR-CORRECTION; V-ANDROMEDAE; STELLAR SPIN
AB We establish the three-dimensional architecture of the Kepler-419 (previously KOI-1474) system to be eccentric yet with a low mutual inclination. Kepler-419b is a warm Jupiter at semi-major axis a = 0.370(-0.006)(+0.007) AU with a large eccentricity (e = 0.85(-0.07)(+0.08)) measured via the "photoeccentric effect." It exhibits transit timing variations (TTVs) induced by the non-transiting Kepler-419c, which we uniquely constrain to be a moderately eccentric (e = 0.184 +/- 0.002), hierarchically separated (a = 1.68 +/- 0.03 AU) giant planet (7.3 +/- 0.4 M-Jup). We combine 16 quarters of Kepler photometry, radial-velocity (RV) measurements from the HIgh Resolution Echelle Spectrometer on Keck, and improved stellar parameters that we derive from spectroscopy and asteroseismology. From the RVs, we measure the mass of the inner planet to be 2.5 +/- 0.3 M-Jup and confirm its photometrically measured eccentricity, refining the value to e = 0.83 +/- 0.01. The RV acceleration is consistent with the properties of the outer planet derived from TTVs. We find that despite their sizable eccentricities, the planets are coplanar to within 9(-6)(+8) degrees, and therefore the inner planet's large eccentricity and close-in orbit are unlikely to be the result of Kozai migration. Moreover, even over many secular cycles, the inner planet's periapse is most likely never small enough for tidal circularization. Finally, we present and measure a transit time and impact parameter from four simultaneous ground-based light curves from 1 m class telescopes, demonstrating the feasibility of ground-based follow-up of Kepler giant planets exhibiting large TTVs.
C1 [Dawson, Rebekah I.; Clubb, Kelsey I.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA.
[Johnson, John Asher; Murray-Clay, Ruth A.] Harvard Smithsonian Ctr Astrophys, Inst Theory & Computat, Cambridge, MA 02138 USA.
[Fabrycky, Daniel C.] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60664 USA.
[Foreman-Mackey, Daniel] NYU, Dept Phys, Ctr Cosmol & Particle Phys, New York, NY 10003 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.
[Cargile, Phillip A.] Vanderbilt Univ, Dept Phys & Astron, Nashville, TN 37235 USA.
[Fulton, Benjamin J.; Howard, Andrew W.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA.
[Hebb, Leslie] Hobart & William Smith Coll, Dept Phys, Geneva, NY 14456 USA.
[Huber, Daniel] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Huber, Daniel] SETI Inst, Mountain View, CA 94043 USA.
[Shporer, Avi] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA.
[Shporer, Avi] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Valenti, Jeff A.] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
RP Dawson, RI (reprint author), Univ Calif Berkeley, Dept Astron, Hearst Field Annex B-20, Berkeley, CA 94720 USA.
EM rdawson@berkeley.edu
RI Howard, Andrew/D-4148-2015;
OI Howard, Andrew/0000-0001-8638-0320; Buchhave, Lars
A./0000-0003-1605-5666; Fabrycky, Daniel/0000-0003-3750-0183
FU Alfred P. Sloan and David and Lucile Packard foundations; NASA
[NNX12AI50G, NNX14AB92G]; National Science Foundation [IIS-1124794];
NASA Postdoctoral Program at Ames Research Center; NASA Science Mission
directorate; Association of Universities for Research in Astronomy,
Inc., under NASA [NAS5-26555]; NASA Office of Space Science
[NNX09AF08G]; W. M. Keck Foundation
FX We are grateful to the referee for a helpful report. We thank David
Hogg, Gongjie Li, Katherine Deck, Joshua Carter, Guillaume Hebrard, Boas
Katz, Yoram Lithwick, Smadar Naoz, Eugene Chiang, Scott Tremaine, Ellen
Price, Leslie Rogers, Eric Ford, Cristobal Petrovich, and Doug Lin for
helpful discussions. R. I. D. gratefully acknowledges the Miller
Institute for Basic Research in Science, University of California
Berkeley. J. A. J. is grateful for the generous grant support provided
by the Alfred P. Sloan and David and Lucile Packard foundations. D. F.
M. is supported by NASA under grant NNX12AI50G and the National Science
Foundation under grant IIS-1124794. D. H. acknowledges support by an
appointment to the NASA Postdoctoral Program at Ames Research Center
administered by Oak Ridge Associated Universities, and NASA Grant
NNX14AB92G issued through the Kepler Participating Scientist Program.
This work benefited from the Summer Program on Modern Statistical and
Computational Methods for Analysis of Kepler Data, held at SAMSI,
Research Triangle Park, NC in 2013 June.; This paper includes data
collected by the Kepler mission. Funding for the Kepler mission is
provided by the NASA Science Mission directorate. We are grateful to the
Kepler Team for their extensive efforts in producing such high-quality
data. Some 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.; We are very grateful to
Geoff Marcy and Howard Isaacson for contributing to the radial-velocity
observations of Kepler-419. J. A. J. is grateful for Keck/HIRES time
allocated through the Caltech Time Allocation Committee for some of the
spectra used herein. The spectroscopic and radial-velocity measurements
presented herein 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 the National Aeronautics
and Space Administration. The Observatory was made possible by the
generous financial support of the W. M. Keck Foundation. We gratefully
acknowledge the efforts and dedication of the Keck Observatory staff,
especially Scott Dahm, Greg Doppman, Hien Tran, and Grant Hill for
support of HIRES and GregWirth for support of remote observing. We
extend special thanks to those of Hawai'ian ancestry on whose sacred
mountain of Mauna Kea we are privileged to be guests. Without their
generous hospitality, the Keck observations presented herein would not
have been possible.
NR 87
TC 21
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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 AUG 20
PY 2014
VL 791
IS 2
AR 89
DI 10.1088/0004-637X/791/2/89
PG 19
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AM7EV
UT WOS:000340028400016
ER
PT J
AU Koenig, XP
Leisawitz, DT
AF Koenig, X. P.
Leisawitz, D. T.
TI A CLASSIFICATION SCHEME FOR YOUNG STELLAR OBJECTS USING THE WIDE-FIELD
INFRARED SURVEY EXPLORER AllWISE CATALOG: REVEALING LOW-DENSITY STAR
FORMATION IN THE OUTER GALAXY
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE circumstellar matter; H II regions; infrared: stars; stars: formation;
stars: pre-main sequence
ID MAIN-SEQUENCE STARS; INTERSTELLAR-MEDIUM; SOLAR NEIGHBORHOOD;
PLANETARY-NEBULAE; MOLECULAR CLOUDS; GALACTIC-CENTER; SPITZER SURVEY;
WISE MISSION; OH/IR STARS; MU-M
AB We present an assessment of the performance of WISE and the AllWISE data release for a section of the Galactic Plane. We lay out an approach to increasing the reliability of point-source photometry extracted from the AllWISE catalog in Galactic Plane regions using parameters provided in the catalog. We use the resulting catalog to construct a new, revised young star detection and classification scheme combining WISE and 2MASS near- and mid-infrared colors and magnitudes and test it in a section of the outer Milky Way. The clustering properties of the candidate Class I and II stars using a nearest neighbor density calculation and the two-point correlation function suggest that the majority of stars do form in massive star-forming regions, and any isolated mode of star formation is at most a small fraction of the total star forming output of the Galaxy. We also show that the isolated component may be very small and could represent the tail end of a single mechanism of star formation in line with models of molecular cloud collapse with supersonic turbulence and not a separate mode all to itself.
C1 [Koenig, X. P.] Yale Univ, Dept Astron, New Haven, CT 06511 USA.
[Leisawitz, D. T.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Koenig, XP (reprint author), Yale Univ, Dept Astron, New Haven, CT 06511 USA.
OI Koenig, Xavier/0000-0002-9478-4170
FU NASA ADAP grant [NNX13AF07G]; National Aeronautics and Space
Administration (NASA); NASA; National Science Foundation
FX We thank the anonymous referee whose comments and suggestions improved
the paper. Author Koenig gratefully acknowledges support from NASA ADAP
grant No. NNX13AF07G. This work is based on data obtained from (1) the
Wide-Field Infrared Survey Explorer, which is a joint project of the
University of California, Los Angeles, and the Jet Propulsion Laboratory
(JPL), California Institute of Technology (Caltech), funded by the
National Aeronautics and Space Administration (NASA); (2) the Two Micron
All Sky Survey, a joint project of the University of Massachusetts and
the Infrared Processing and Analysis Center (IPAC)/Caltech, funded by
NASA and the National Science Foundation; and (3) the NASA/IPAC Infrared
Science Archive, which is operated by JPL, Caltech, under a contract
with NASA. This research has made use of NASA's Astrophysics Data
System.
NR 61
TC 18
Z9 18
U1 0
U2 0
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 AUG 20
PY 2014
VL 791
IS 2
AR 131
DI 10.1088/0004-637X/791/2/131
PG 27
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AM7EV
UT WOS:000340028400058
ER
PT J
AU Masiero, JR
Grav, T
Mainzer, AK
Nugent, CR
Bauer, JM
Stevenson, R
Sonnett, S
AF Masiero, Joseph R.
Grav, T.
Mainzer, A. K.
Nugent, C. R.
Bauer, J. M.
Stevenson, R.
Sonnett, S.
TI MAIN-BELT ASTEROIDS WITH WISE/NEOWISE: NEAR-INFRARED ALBEDOS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE minor planets, asteroids: general
ID SURVEY-EXPLORER; THERMAL-MODEL; SOLAR-SYSTEM; NEOWISE; IDENTIFICATION;
METEORITES; FAMILIES; ORGANICS; MISSION; SURFACE
AB We present revised near-infrared albedo fits of 2835 main-belt asteroids observed by WISE/NEOWISE over the course of its fully cryogenic survey in 2010. These fits are derived from reflected-light near-infrared images taken simultaneously with thermal emission measurements, allowing for more accurate measurements of the near-infrared albedos than is possible for visible albedo measurements. Because our sample requires reflected light measurements, it undersamples small, low-albedo asteroids, as well as those with blue spectral slopes across the wavelengths investigated. We find that the main belt separates into three distinct groups of 6%, 16%, and 40% reflectance at 3.4 mu m. Conversely, the 4.6 mu m albedo distribution spans the full range of possible values with no clear grouping. Asteroid families show a narrow distribution of 3.4 m albedos within each family that map to one of the three observed groupings, with the (221) Eos family being the sole family associated with the 16% reflectance 3.4 m albedo group. We show that near-infrared albedos derived from simultaneous thermal emission and reflected light measurements are important indicators of asteroid taxonomy and can identify interesting targets for spectroscopic follow-up.
C1 [Masiero, Joseph R.; Mainzer, A. K.; Nugent, C. R.; Bauer, J. M.; Stevenson, R.; Sonnett, S.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Grav, T.] Planetary Sci Inst, Tucson, AZ USA.
[Bauer, J. M.] CALTECH, Ctr Infrared Proc & Anal, Pasadena, CA 91125 USA.
RP Masiero, JR (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr,MS 183-601, Pasadena, CA 91109 USA.
EM Joseph.Masiero@jpl.nasa.gov; tgrav@psi.edu; amainzer@jpl.nasa.gov;
cnugent@jpl.nasa.gov; James.Bauer@jpl.nasa.gov;
Rachel.A.Stevenson@jpl.nasa.gov; sarah.sonnett@jpl.nasa.gov
OI Masiero, Joseph/0000-0003-2638-720X
FU NASA Planetary Geology and Geophysics grant; National Aeronautics and
Space Administration; Planetary Science Division of the National
Aeronautics and Space Administration
FX J.M. was partially supported by a NASA Planetary Geology and Geophysics
grant. C.N., R. S., and S. S. were supported by an appointment to the
NASA Postdoctoral Program at JPL, administered by Oak Ridge Associated
Universities through a contract with NASA. We thank the referee for
helpful comments that greatly improved this manuscript. This publication
makes use of data products from the Wide-field 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
publication also makes use of data products from NEOWISE, which is a
project of the Jet Propulsion Laboratory/California Institute of
Technology, funded by the Planetary Science Division of the National
Aeronautics and Space Administration. This research has made use of the
NASA/IPAC Infrared Science Archive, which is operated by the Jet
Propulsion Laboratory, California Institute of Technology, under
contract with the National Aeronautics and Space Administration.
NR 39
TC 16
Z9 16
U1 0
U2 5
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 AUG 20
PY 2014
VL 791
IS 2
AR 121
DI 10.1088/0004-637X/791/2/121
PG 11
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AM7EV
UT WOS:000340028400048
ER
PT J
AU Paganini, L
Mumma, MJ
Villanueva, GL
Keane, JV
Blake, GA
Bonev, BP
DiSanti, MA
Gibb, EL
Meech, KJ
AF Paganini, L.
Mumma, M. J.
Villanueva, G. L.
Keane, J. V.
Blake, G. A.
Bonev, B. P.
DiSanti, M. A.
Gibb, E. L.
Meech, K. J.
TI C/2013 R1 (LOVEJOY) AT IR WAVELENGTHS AND THE VARIABILITY OF CO
ABUNDANCES AMONG OORT CLOUD COMETS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE astrochemistry; comets: general; comets: individual (C/2013 R1
(Lovejoy)); infrared: planetary systems; molecular processes; Oort Cloud
ID O1 HALE-BOPP; HUBBLE-SPACE-TELESCOPE; C/1996 B2 HYAKUTAKE;
CARBON-MONOXIDE; CHEMICAL-COMPOSITION; INFRARED WAVELENGTHS; ORGANIC
COMPOSITION; PARENT VOLATILES; Q2 MACHHOLZ; P1 GARRADD
AB We report production rates, rotational temperatures, and related parameters for gases in C/2013 R1 (Lovejoy) using the Near InfraRed SPECtrometer at the Keck Observatory, on six UT dates spanning heliocentric distances (Rh) that decreased from 1.35 AU to 1.16 AU (pre-perihelion). We quantified nine gaseous species (H2O, OH*, CO, CH4, HCN, C2H6, CH3OH, NH3, and NH2) and obtained upper limits for two others (C2H2 and H2CO). Compared with organics-normal comets, our results reveal highly enriched CO, (at most) slightly enriched CH3OH, C2H6, and HCN, and CH4 consistent with " normal", yet depleted, NH3, C2H2, and H2CO. Rotational temperatures increased from similar to 50 K to similar to 70 K with decreasing Rh, following a power law in Rh of -2.0 +/- 0.2, while the water production rate increased from 1.0 to 3.9x1028 molecules s(-1), following a power law in Rh of-4.7 +/- 0.9. The ortho-para ratio for H2O was 3.01 +/- 0.49, corresponding to spin temperatures (Tspin) similar to 29 K (at the 1s level). The observed spatial profiles for these emissions showed complex structures, possibly tied to nucleus rotation, although the cadence of our observations limits any definitive conclusions. The retrieved CO abundance in Lovejoy is more than twice the median value for comets in our IR survey, suggesting this comet is enriched in CO. We discuss the enriched value for CO in comet C/2013 R1 in terms of the variability of CO among Oort Cloud comets.
C1 [Paganini, L.; Mumma, M. J.; Villanueva, G. L.; Bonev, B. P.; DiSanti, M. A.] NASA GSFC, Goddard Ctr Astrobiol, Greenbelt, MD 20771 USA.
[Paganini, L.; Villanueva, G. L.; Bonev, B. P.] Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA.
[Keane, J. V.; Meech, K. J.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA.
[Keane, J. V.; Meech, K. J.] NASA Astrobiol Inst, Mountain View, CA USA.
[Blake, G. A.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA.
[Gibb, E. L.] Univ Missouri, Dept Phys & Astron, St Louis, MO 63121 USA.
RP Paganini, L (reprint author), NASA GSFC, Goddard Ctr Astrobiol, MS 690, Greenbelt, MD 20771 USA.
EM lucas.paganini@nasa.gov
FU NASA's PAST Program; NAI through its member Teams at GSFC; UH
[NNA09DA77A]; NSF [1211362]
FX We gratefully acknowledge support by NASA's PAST Program (L. P., M.J.M,
M. A. D., G. L. V.) and NAI through its member Teams at GSFC (M.J.M., M.
A. D., B. P. B., G. A. B.) and at UH (J.V.K., K.J.M.; No. NNA09DA77A),
and NSF (B. P. B., E. L. G.; Award 1211362). The data of October 24 and
25 were collected during part of the NASA Keck time awarded for
observations of comet ISON, and are publicly available through the Keck
Observatory Archive. We thank the anonymous referee for useful insights
on this paper. The authors 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 67
TC 8
Z9 8
U1 0
U2 5
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 AUG 20
PY 2014
VL 791
IS 2
AR 122
DI 10.1088/0004-637X/791/2/122
PG 8
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AM7EV
UT WOS:000340028400049
ER
PT J
AU Tendulkar, SP
Yang, CW
An, HJ
Kaspi, VM
Archibald, AM
Bassa, C
Bellm, E
Bogdanov, S
Harrison, FA
Hessels, JWT
Janssen, GH
Lyne, AG
Patruno, A
Stappers, B
Stern, D
Tomsick, JA
Boggs, SE
Chakrabarty, D
Christensen, FE
Craig, WW
Hailey, CA
Zhang, W
AF Tendulkar, Shriharsh P.
Yang, Chengwei
An, Hongjun
Kaspi, Victoria M.
Archibald, Anne M.
Bassa, Cees
Bellm, Eric
Bogdanov, Slavko
Harrison, Fiona A.
Hessels, Jason W. T.
Janssen, Gemma H.
Lyne, Andrew G.
Patruno, Alessandro
Stappers, Benjamin
Stern, Daniel
Tomsick, John A.
Boggs, Steven E.
Chakrabarty, Deepto
Christensen, Finn E.
Craig, William W.
Hailey, Charles A.
Zhang, William
TI NuSTAR OBSERVATIONS OF THE STATE TRANSITION OF MILLISECOND PULSAR BINARY
PSR J1023+0038
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE pulsars: general; pulsars: individual (PSR J1023+0038); stars: neutron;
X-rays: stars
ID X-RAY BINARY; QUASI-PERIODIC OSCILLATIONS; 1ST J102347.6+003841;
ACCRETION POWER; XSS J12270-4859; RADIO PULSARS; SPIN-DOWN; SYSTEM;
EMISSION; ROTATION
AB We report NuSTAR observations of the millisecond pulsar-low-mass X-ray binary (LMXB) transition system PSR J1023+0038 from 2013 June and October, before and after the formation of an accretion disk around the neutron star. Between June 10 and 12, a few days to two weeks before the radio disappearance of the pulsar, the 3-79 keV X-ray spectrum was well fit by a simple power law with a photon index of Gamma = 1.17(-0.07)(+0.08) (at 90% confidence) with a 3-79 keV luminosity of 7.4 +/- 0.4 x 10(32) erg s(-1). Significant orbital modulation was observed with a modulation fraction of 36% +/- 10%. During the October 19-21 observation, the spectrum is described by a softer power law (Gamma = 1.66(-0.05)(+0.06)) with an average luminosity of 5.8 +/- 0.2x10(33) erg s(-1) and a peak luminosity of approximate to 1.2x10(34) erg s(-1) observed during a flare. No significant orbital modulation was detected. The spectral observations are consistent with previous and current multiwavelength observations and show the hard X-ray power law extending to 79 keV without a spectral break. Sharp-edged, flat-bottomed dips are observed with widths between 30 and 1000 s and ingress and egress timescales of 30-60 s. No change in hardness ratio was observed during the dips. Consecutive dip separations are log-normal in distribution with a typical separation of approximately 400 s. These dips are distinct from dipping activity observed in LMXBs. We compare and contrast these dips to observations of dips and state changes in the similar transition systems PSR J1824-2452I and XSS J1227.0-4859 and discuss possible interpretations based on the transitions in the inner disk.
C1 [Tendulkar, Shriharsh P.; Bellm, Eric; Harrison, Fiona A.] CALTECH, Pasadena, CA 91125 USA.
[Yang, Chengwei; An, Hongjun; Kaspi, Victoria M.] McGill Univ, Dept Phys, Montreal II3A 2T8, PQ, Canada.
[Yang, Chengwei] Chinese Acad Sci, Natl Space Sci Ctr, Beijing 100190, Peoples R China.
[Archibald, Anne M.; Bassa, Cees; Hessels, Jason W. T.; Janssen, Gemma H.; Patruno, Alessandro] ASTRON, Netherlands Inst Radio Astron, NL-7990 AA Dwingeloo, Netherlands.
[Bogdanov, Slavko; Hailey, Charles A.] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA.
[Hessels, Jason W. T.] Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1090 GE Amsterdam, Netherlands.
[Lyne, Andrew G.; Stappers, Benjamin] Univ Manchester, Sch Phys & Astron, Jodrell Bank Ctr Astrophys, Manchester M13 9PL, Lancs, England.
[Patruno, Alessandro] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands.
[Stern, Daniel] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Tomsick, John A.; Boggs, Steven E.; Craig, William W.] Univ Calif, Space Sci Lab, Berkeley, CA 94720 USA.
[Chakrabarty, Deepto] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA.
[Christensen, Finn E.] Tech Univ Denmark, DTU Space, Natl Space Inst, DK-2800 Lyngby, Denmark.
[Craig, William W.] Lawrence Livermore Natl Lab, Livermore, CA 94550 USA.
[Zhang, William] NASA Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA.
RP Tendulkar, SP (reprint author), CALTECH, 1200 E Calif Blvd,MC 249-17, Pasadena, CA 91125 USA.
EM spt@astro.caltech.edu
RI Boggs, Steven/E-4170-2015;
OI Boggs, Steven/0000-0001-9567-4224; Bellm, Eric/0000-0001-8018-5348; An,
Hongjun/0000-0002-6389-9012; Archibald, Anne/0000-0003-0638-3340
FU NASA [NNG08FD60C]; NuSTAR mission; California Institute of Technology;
National Aeronautics and Space Administration; NSERC Discovery Grant;
Centre de Recherche en Astrophysique du Quebec, an R. Howard Webster
Foundation Fellowship from the Canadian Institute for Advanced Study;
Canada Research Chairs Program; Lorne Trottier Chair in Astrophysics and
Cosmology; ERC starting grant DRAGNET; Netherlands Organization for
Scientic Research (NWO) Vidi fellowship
FX We thank the anonymous referee for detailed suggestions and comments.
This work was supported under NASA Contract No. NNG08FD60C and made use
of data from the NuSTAR mission, a project led by the California
Institute of Technology, managed by the Jet Propulsion Laboratory, and
funded by the National Aeronautics and Space Administration. We thank
the NuSTAR Operations, Software, and Calibration teams for support with
the execution and analysis of these observations. This research made use
of the NuSTAR Data Analysis Software (NuSTARDAS) jointly developed by
the ASI Science Data Center (ASDC, Italy) and the California Institute
of Technology (USA). VMKreceives support from an NSERC Discovery Grant
and Accelerator Supplement, from the Centre de Recherche en
Astrophysique du Quebec, an R. Howard Webster Foundation Fellowship from
the Canadian Institute for Advanced Study, the Canada Research Chairs
Program, and the Lorne Trottier Chair in Astrophysics and Cosmology. J.
W. T. H. acknowledges funding for this work from ERC starting grant
DRAGNET. A. P. acknowledges support from the Netherlands Organization
for Scientic Research (NWO) Vidi fellowship.
NR 52
TC 20
Z9 20
U1 1
U2 5
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 AUG 20
PY 2014
VL 791
IS 2
AR 77
DI 10.1088/0004-637X/791/2/77
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AM7EV
UT WOS:000340028400004
ER
PT J
AU Wang, J
Fischer, DA
Xie, JW
Ciardi, DR
AF Wang, Ji
Fischer, Debra A.
Xie, Ji-Wei
Ciardi, David R.
TI INFLUENCE OF STELLAR MULTIPLICITY ON PLANET FORMATION. II. PLANETS ARE
LESS COMMON IN MULTIPLE-STAR SYSTEMS WITH SEPARATIONS SMALLER THAN 1500
AU
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE methods: observational; methods: statistical; planetary systems; planets
and satellites: fundamental parameters; techniques: high angular
resolution; techniques: photometric
ID EXOPLANET HOST STARS; TRANSITING CIRCUMBINARY PLANET; RADIAL-VELOCITY
SEARCH; SOLAR-TYPE STARS; ADAPTIVE OPTICS; BINARY-SYSTEMS; EXTRASOLAR
PLANETS; HABITABLE ZONES; INFRARED CAMERA; KEPLER OBJECTS
AB Almost half of the stellar systems in the solar neighborhood are made up of multiple stars. In multiple-star systems, planet formation is under the dynamical influence of stellar companions, and the planet occurrence rate is expected to be different from that of single stars. There have been numerous studies on the planet occurrence rate of single star systems. However, to fully understand planet formation, the planet occurrence rate in multiple-star systems needs to be addressed. In this work, we infer the planet occurrence rate in multiple-star systems by measuring the stellar multiplicity rate for planet host stars. For a subsample of 56 Kepler planet host stars, we use adaptive optics (AO) imaging and the radial velocity (RV) technique to search for stellar companions. The combination of these two techniques results in high search completeness for stellar companions. We detect 59 visual stellar companions to 25 planet host stars with AO data. Three stellar companions are within 2 '' and 27 within 6 ''. We also detect two possible stellar companions (KOI 5 and KOI 69) showing long-term RV acceleration. After correcting for a bias against planet detection in multiple-star systems due to flux contamination, we find that planet formation is suppressed in multiple-star systems with separations smaller than 1500 AU. Specifically, we find that compared to single star systems, planets in multiple-star systems occur 4.5 +/- 3.2, 2.6 +/- 1.0, and 1.7 +/- 0.5 times less frequently when a stellar companion is present at a distance of 10, 100, and 1000 AU, respectively. This conclusion applies only to circumstellar planets; the planet occurrence rate for circumbinary planets requires further investigation.
C1 [Wang, Ji; Fischer, Debra A.] Yale Univ, Dept Astron, New Haven, CT 06511 USA.
[Xie, Ji-Wei] Nanjing Univ, Minist Educ, Dept Astron, Nanjing 210093, Jiangsu, Peoples R China.
[Xie, Ji-Wei] Nanjing Univ, Minist Educ, Key Lab Modern Astron & Astrophys, Nanjing 210093, Jiangsu, Peoples R China.
[Ciardi, David R.] NASA, Exoplanet Sci Inst, CALTECH, Pasadena, CA 91125 USA.
RP Wang, J (reprint author), Yale Univ, Dept Astron, New Haven, CT 06511 USA.
EM ji.wang@yale.edu
OI Ciardi, David/0000-0002-5741-3047; Wang, Ji/0000-0002-4361-8885
FU Foundation for the Author of National Excellent Doctoral Dissertation
(FANEDD) of PR China
FX The authors thank Howard Isaacson and Matt Giguere for helpful comments
and proofreading the paper. The research is made possible by the data
from the Kepler Community Followup Observing Program (CFOP). The authors
acknowledge all the CFOP users who uploaded the AO and RV data used in
the paper. This research has 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. Ji-wei Xie is supported by a
Foundation for the Author of National Excellent Doctoral Dissertation
(FANEDD) of PR China.
NR 81
TC 40
Z9 40
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 AUG 20
PY 2014
VL 791
IS 2
AR 111
DI 10.1088/0004-637X/791/2/111
PG 16
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AM7EV
UT WOS:000340028400038
ER
PT J
AU Andreev-Andrievskiy, A
Popova, A
Boyle, R
Alberts, J
Shenkman, B
Vinogradova, O
Dolgov, O
Anokhin, K
Tsvirkun, D
Soldatov, P
Nemirovskaya, T
Ilyin, E
Sychev, V
AF Andreev-Andrievskiy, Alexander
Popova, Anfisa
Boyle, Richard
Alberts, Jeffrey
Shenkman, Boris
Vinogradova, Olga
Dolgov, Oleg
Anokhin, Konstantin
Tsvirkun, Darya
Soldatov, Pavel
Nemirovskaya, Tatyana
Ilyin, Eugeniy
Sychev, Vladimir
TI Mice in Bion-M 1 Space Mission: Training and Selection
SO PLOS ONE
LA English
DT Article
ID ENVIRONMENTAL ENRICHMENT; LABORATORY MICE; INBRED MICE; HEART-RATE;
STRESS; SPACEFLIGHT; MOUSE; SUSCEPTIBILITY; RESPONSES; STRENGTH
AB After a 16-year hiatus, Russia has resumed its program of biomedical research in space, with the successful 30-day flight of the Bion-M 1 biosatellite (April 19-May 19, 2013). The principal species for biomedical research in this project was the mouse. This paper presents an overview of the scientific goals, the experimental design and the mouse training/selection program. The aim of mice experiments in the Bion-M 1 project was to elucidate cellular and molecular mechanisms, underlying the adaptation of key physiological systems to long-term exposure in microgravity. The studies with mice combined in vivo measurements, both in flight and post-flight (including continuous blood pressure measurement), with extensive in vitro studies carried out shortly after return of the mice and in the end of recovery study. Male C57/BL6 mice group housed in space habitats were flown aboard the Bion-M 1 biosatellite, or remained on ground in the control experiment that replicated environmental and housing conditions in the spacecraft. Vivarium control groups were used to account for housing effects and possible seasonal differences. Mice training included the co-adaptation in housing groups and mice adaptation to paste food diet. The measures taken to co-adapt aggressive male mice in housing groups and the peculiarities of "space'' paste food are described. The training program for mice designated for in vivo studies was broader and included behavioral/functional test battery and continuous behavioral measurements in the home-cage. The results of the preliminary tests were used for the selection of homogenous groups. After the flight, mice were in good condition for biomedical studies and displayed signs of pronounced disadaptation to Earth's gravity. The outcomes of the training program for the mice welfare are discussed. We conclude that our training program was effective and that male mice can be successfully employed in space biomedical research.
C1 [Andreev-Andrievskiy, Alexander; Popova, Anfisa; Shenkman, Boris; Vinogradova, Olga; Tsvirkun, Darya; Soldatov, Pavel; Nemirovskaya, Tatyana; Ilyin, Eugeniy; Sychev, Vladimir] Russian Acad Sci, Inst Biomed Problems, Moscow, Russia.
[Andreev-Andrievskiy, Alexander; Popova, Anfisa] Moscow MV Lomonosov State Univ, Fac Biol, Moscow, Russia.
[Boyle, Richard] NASA, Ames Res Ctr, Biovisualizat Imaging & Simulat Technol Ctr BioVI, Moffett Field, CA 94035 USA.
[Alberts, Jeffrey] Indiana Univ, Dept Psychol & Brain Sci, Bloomington, IN USA.
[Dolgov, Oleg; Anokhin, Konstantin] Russian Acad Med Sci, Anokhin Inst Normal Physiol, Moscow, Russia.
[Anokhin, Konstantin] Kurchatov Inst, Kurchatov NBIC Ctr, Natl Res Ctr, Moscow, Russia.
RP Andreev-Andrievskiy, A (reprint author), Russian Acad Sci, Inst Biomed Problems, Moscow, Russia.
EM aandrievsky@gmail.com
RI Andreev-Andrievskiy, Alexander/B-7336-2013
OI Andreev-Andrievskiy, Alexander/0000-0002-1173-8153
FU Russian Federal Space Agency; Russian Academy of Sciences; Division of
Physiology and Fundamental Medicine of Russian Academy of Sciences; RFBR
[12-04-01665-a]
FX The project was supported by the Russian Federal Space Agency and the
Russian Academy of Sciences. These funders took part in study design and
data collection, but had no role in data analysis or decision to
publish. The study was also supported by the Division of Physiology and
Fundamental Medicine of Russian Academy of Sciences ("Integrative
physiology" program) and RFBR grant 12-04-01665-a. These funders had no
role in study design, data collection and analysis, decision to publish,
or preparation of the manuscript.
NR 36
TC 10
Z9 10
U1 1
U2 12
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 AUG 18
PY 2014
VL 9
IS 8
AR e104830
DI 10.1371/journal.pone.0104830
PG 15
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA AO4JF
UT WOS:000341302700043
PM 25133741
ER
PT J
AU Cable, ML
Vu, TH
Hodyss, R
Choukroun, M
Malaska, MJ
Beauchamp, P
AF Cable, Morgan L.
Vu, Tuan H.
Hodyss, Robert
Choukroun, Mathieu
Malaska, Michael J.
Beauchamp, Patricia
TI Experimental determination of the kinetics of formation of the
benzene-ethane co-crystal and implications for Titan
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
DE ethane; benzene; cocrystal; evaporite; hydrocarbon; Titan
ID CHEMICAL-COMPOSITION; ATMOSPHERE; SPECTRA; DRIZZLE; LAKES
AB Benzene is found on Titan and is a likely constituent of the putative evaporite deposits formed around the hydrocarbon lakes. We have recently demonstrated the formation of a benzene-ethane co-crystal under Titan-like surface conditions. Here we investigate the kinetics of formation of this new structure as a function of temperature. We show that the formation process would reach completion under Titan surface conditions in similar to 18 h and that benzene precipitates from liquid ethane as the co-crystal. This suggests that benzene-rich evaporite basins around ethane/methane lakes and seas may not contain pure crystalline benzene, but instead benzene-ethane co-crystals. This co-crystalline form of benzene with ethane represents a new class of materials for Titan's surface, analogous to hydrated minerals on Earth. This new structure may also influence evaporite characteristics such as particle size, dissolution rate, and infrared spectral properties.
C1 [Cable, Morgan L.; Vu, Tuan H.; Hodyss, Robert; Choukroun, Mathieu; Malaska, Michael J.; Beauchamp, Patricia] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
RP Hodyss, R (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
EM Robert.P.Hodyss@jpl.nasa.gov
RI Choukroun, Mathieu/F-3146-2017; Vu, Tuan/F-5223-2017;
OI Choukroun, Mathieu/0000-0001-7447-9139; Vu, Tuan/0000-0001-6839-9765;
Malaska, Michael/0000-0003-0064-5258
FU NASA Astrobiology Institute, Titan as a Prebiotic Chemical System; NASA
Outer Planets Research (OPR) Program; NASA's Outer Planets Research
Program; NASA Postdoctoral Program; NASA
FX We thank Ralph Lorenz and Jason Barnes for helpful comments. M. L. C.,
M. C., P. B., and R. H. were funded by the NASA Astrobiology Institute,
Titan as a Prebiotic Chemical System. TV was funded through the NASA
Outer Planets Research (OPR) Program. M. M. was funded through NASA's
Outer Planets Research Program and the NASA Postdoctoral Program,
administered by Oak Ridge Associated Universities through a contract
with NASA. This work was carried out at the Jet Propulsion Laboratory,
California Institute of Technology, under contract with NASA. Data
reported in this work may be accessed by contacting the corresponding
author. Government sponsorship is gratefully acknowledged.
NR 27
TC 2
Z9 2
U1 2
U2 22
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 AUG 16
PY 2014
VL 41
IS 15
BP 5396
EP 5401
DI 10.1002/2014GL060531
PG 6
WC Geosciences, Multidisciplinary
SC Geology
GA AP0BI
UT WOS:000341725200011
ER
PT J
AU Dutrieux, P
Stewart, C
Jenkins, A
Nicholls, KW
Corr, HFJ
Rignot, E
Steffen, K
AF Dutrieux, Pierre
Stewart, Craig
Jenkins, Adrian
Nicholls, Keith W.
Corr, Hugh F. J.
Rignot, Eric
Steffen, Konrad
TI Basal terraces on melting ice shelves
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
DE cryosphere; ice shelf-ocean interactions; ocean; ice
ID PINE ISLAND GLACIER; PHASE-SENSITIVE RADAR; WEST ANTARCTICA; BENEATH;
SHEET; RETREAT; CIRCULATION; CHANNELS; MODEL; WATER
AB Ocean waters melt the margins of Antarctic and Greenland glaciers, and individual glaciers' responses and the integrity of their ice shelves are expected to depend on the spatial distribution of melt. The bases of the ice shelves associated with Pine Island Glacier (West Antarctica) and Petermann Glacier (Greenland) have similar geometries, including kilometer-wide, hundreds-of-meter high channels oriented along and across the direction of ice flow. The channels are enhanced by, and constrain, oceanic melt. New meter-scale observations of basal topography reveal peculiar glaciated landscapes. Channel flanks are not smooth, but are instead stepped, with hundreds-of-meters-wide flat terraces separated by 5-50m high walls. Melting is shown to be modulated by the geometry: constant across each terrace, changing from one terrace to the next, and greatly enhanced on the similar to 45 degrees inclined walls. Melting is therefore fundamentally heterogeneous and likely associated with stratification in the ice-ocean boundary layer, challenging current models of ice shelf-ocean interactions.
C1 [Dutrieux, Pierre; Jenkins, Adrian; Nicholls, Keith W.; Corr, Hugh F. J.] British Antarctic Survey, NERC, Cambridge, England.
[Stewart, Craig] Univ Cambridge, Scott Polar Res Inst, Cambridge CB2 1ER, England.
[Rignot, Eric] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Rignot, Eric] Univ Calif Irvine, Dept Earth Syst Sci, Irvine, CA USA.
[Steffen, Konrad] Swiss Fed Res Inst WLS, Birmensdorf, Switzerland.
[Steffen, Konrad] Swiss Fed Inst Technol, Inst Atmosphere & Climate, Zurich, Switzerland.
RP Dutrieux, P (reprint author), British Antarctic Survey, NERC, Cambridge, England.
EM pierre.dutrieux@bas.ac.uk
RI Steffen, Konrad/C-6027-2013; Rignot, Eric/A-4560-2014; Dutrieux,
Pierre/B-7568-2012
OI Steffen, Konrad/0000-0001-8658-1026; Rignot, Eric/0000-0002-3366-0481;
Dutrieux, Pierre/0000-0002-8066-934X
FU NERC [NE/G001367/1, NE/J005770/1]; NSF [NAG5-12075]; NASA grant,
Cryopshere Science Program
FX P.D. was supported by the NERC grants NE/G001367/1 and NE/J005770/1.
Stanley S. Jacobs and NSF are acknowledged for providing shipboard
support during the Autosub observations. Stephen D. McPhail, James R.
Perrett, Andrew T. Webb, and David White are acknowledged for
configuring and preparing the Autosub missions. Field work on Petermann
glacier was supported by the NSF grant NAG5-12075 and a NASA grant from
the Cryopshere Science Program. The data used to produce the results of
this paper are freely available upon request to the authors.
NR 39
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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 AUG 16
PY 2014
VL 41
IS 15
BP 5506
EP 5513
DI 10.1002/2014GL060618
PG 8
WC Geosciences, Multidisciplinary
SC Geology
GA AP0BI
UT WOS:000341725200025
ER
PT J
AU Carlson, AE
Winsor, K
Ullman, DJ
Brook, EJ
Rood, DH
Axford, Y
LeGrande, AN
Anslow, FS
Sinclair, G
AF Carlson, Anders E.
Winsor, Kelsey
Ullman, David J.
Brook, Edward J.
Rood, Dylan H.
Axford, Yarrow
LeGrande, Allegra N.
Anslow, Faron S.
Sinclair, Gaylen
TI Earliest Holocene south Greenland ice sheet retreat within its late
Holocene extent
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
DE Greenland ice sheet; cosmogenic dating; early Holocene climate
ID PRODUCTION-RATE CALIBRATION; SEA-LEVEL CHANGES; WEST GREENLAND;
LAKE-SEDIMENTS; JAKOBSHAVN-ISFJORD; CLIMATE VARIATIONS; HISTORY; BE-10;
TEMPERATURE; MAXIMUM
AB Early Holocene summer warmth drove dramatic Greenland ice sheet (GIS) retreat. Subsequent insolation-driven cooling caused GIS margin readvance to late Holocene maxima, from which ice margins are now retreating. We use Be-10 surface exposure ages from four locations between 69.4 degrees N and 61.2 degrees N to date when in the early Holocene south to west GIS margins retreated to within these late Holocene maximum extents. We find that this occurred at 11.10.2 ka to 10.60.5 ka in south Greenland, significantly earlier than previous estimates, and 6.80.1 ka to 7.90.1 ka in southwest to west Greenland, consistent with existing Be-10 ages. At least in south Greenland, these Be-10 ages likely provide a minimum constraint for when on a multicentury timescale summer temperatures after the last deglaciation warmed above late Holocene temperatures in the early Holocene. Current south Greenland ice margin retreat suggests that south Greenland may have now warmed to or above earliest Holocene summer temperatures.
C1 [Carlson, Anders E.; Ullman, David J.; Brook, Edward J.; Sinclair, Gaylen] Oregon State Univ, Coll Earth Ocean & Atmospher Sci, Corvallis, OR 97331 USA.
[Winsor, Kelsey] Univ Wisconsin, Dept Geosci, Madison, WI USA.
[Rood, Dylan H.] Univ Glasgow, Scottish Univ Environm Res Ctr, Glasgow, Lanark, Scotland.
[Rood, Dylan H.] Univ Calif Santa Barbara, Earth Res Inst, Santa Barbara, CA 93106 USA.
[Axford, Yarrow] Northwestern Univ, Dept Earth & Planetary Sci, Evanston, IL USA.
[LeGrande, Allegra N.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
[LeGrande, Allegra N.] Columbia Univ, Ctr Climate Syst Res, New York, NY USA.
[Anslow, Faron S.] Univ Victoria, Pacific Climate Impacts Consortium, Victoria, BC, Canada.
RP Carlson, AE (reprint author), Oregon State Univ, Coll Earth Ocean & Atmospher Sci, Corvallis, OR 97331 USA.
EM acarlson@coas.oregonstate.edu
RI Axford, Yarrow/N-4151-2014
OI Axford, Yarrow/0000-0002-8033-358X
FU National Geographic Society [8687-09]
FX We thank D. Murray, J. Harvey, B. Goehring, and S. Marcott for lab
assistance, S. Marcott for discussion of the Northern Hemisphere
temperature stack, N. Larsen for sharing data, and the National
Geographic Society (award 8687-09 to A.E. Carlson). Comments by two
anonymous reviewers significantly improved this manuscript. Data are
available in Tables S1 and S2.
NR 55
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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 AUG 16
PY 2014
VL 41
IS 15
BP 5514
EP 5521
DI 10.1002/2014GL060800
PG 8
WC Geosciences, Multidisciplinary
SC Geology
GA AP0BI
UT WOS:000341725200026
ER
PT J
AU Allan, RP
Liu, CL
Loeb, NG
Palmer, MD
Roberts, M
Smith, D
Vidale, PL
AF Allan, Richard P.
Liu, Chunlei
Loeb, Norman G.
Palmer, Matthew D.
Roberts, Malcolm
Smith, Doug
Vidale, Pier-Luigi
TI Changes in global net radiative imbalance 1985-2012
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
DE radiative flux; climate variability; satellite data; climate model;
energy balance; temperature
ID CLIMATE-CHANGE; DECADAL VARIABILITY; WARMING HIATUS; ENERGY BUDGET;
WATER-VAPOR; MODEL; TEMPERATURE; SYSTEM; CMIP5; EARTH
AB Combining satellite data, atmospheric reanalyses, and climate model simulations, variability in the net downward radiative flux imbalance at the top of Earth's atmosphere (N) is reconstructed and linked to recent climate change. Over the 1985-1999 period mean N (0.34 0.67Wm(-2)) is lower than for the 2000-2012 period (0.62 0.43Wm(-2), uncertainties at 90% confidence level) despite the slower rate of surface temperature rise since 2000. While the precise magnitude of N remains uncertain, the reconstruction captures interannual variability which is dominated by the eruption of Mount Pinatubo in 1991 and the El Nino Southern Oscillation. Monthly deseasonalized interannual variability in N generated by an ensemble of nine climate model simulations using prescribed sea surface temperature and radiative forcings and from the satellite-based reconstruction is significantly correlated (r approximate to 0.6) over the 1985-2012 period.
C1 [Allan, Richard P.; Liu, Chunlei; Vidale, Pier-Luigi] Univ Reading, Dept Meteorol, Reading, Berks, England.
[Loeb, Norman G.] NASA, Langley Res Ctr, Hampton, VA 23665 USA.
[Palmer, Matthew D.; Roberts, Malcolm; Smith, Doug] Met Off, Exeter, Devon, England.
RP Allan, RP (reprint author), Univ Reading, Dept Meteorol, Reading, Berks, England.
EM r.p.allan@reading.ac.uk
RI Allan, Richard/B-5782-2008;
OI Allan, Richard/0000-0003-0264-9447; Vidale, Pier
Luigi/0000-0002-1800-8460
FU Natural Environment Research Council (NERC) DEEP-C [NE/K005480/1];
National Centre for Atmospheric Science; National Centre for Earth
Observation
FX This work was supported by the Natural Environment Research Council
(NERC) DEEP-C grant NE/K005480/1, the National Centre for Atmospheric
Science, and the National Centre for Earth Observation. 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 (models listed in Table 1) for producing and making
available their model outputs; for CMIP, the U.S. Department of Energy's
PCMDI provided coordinating support and led development of software
infrastructure in partnership with the Global Organization for Earth
System Science Portals. The UPSCALE simulations were performed under a
grant of supercomputing time from PRACE using the HLRS HERMIT Cray XE6.
Data generated by this work are available at
http://www.met.reading.ac.uk/similar to sgs02rpa/research/DEEP-C/GRL/.
We thank Kevin Trenberth and Kyle Armour for taking the time to review
our work, which helped to improve the manuscript.
NR 57
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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 AUG 16
PY 2014
VL 41
IS 15
BP 5588
EP 5597
DI 10.1002/2014GL060962
PG 10
WC Geosciences, Multidisciplinary
SC Geology
GA AP0BI
UT WOS:000341725200035
ER
PT J
AU Xi, BK
Dong, XQ
Minnis, P
Sun-Mack, S
AF Xi, Baike
Dong, Xiquan
Minnis, Patrick
Sun-Mack, Sunny
TI Comparison of marine boundary layer cloud properties from CERES-MODIS
Edition 4 and DOE ARM AMF measurements at the Azores
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
ID GROUND-BASED MEASUREMENTS; ENERGY SYSTEM CERES; LIQUID WATER PATH;
STRATOCUMULUS CLOUD; SATELLITE-OBSERVATIONS; CLIMATE; RETRIEVALS; TERRA;
AQUA; FRACTION
AB Marine boundary layer (MBL) cloud properties derived from the NASA Clouds and the Earth's Radiant Energy System (CERES) project using Terra and Aqua Moderate Resolution Imaging Spectroradiometer (MODIS) data are compared with observations taken at the Department of Energy Atmospheric Radiation Measurement (ARM) Mobile Facility at the Azores (AMF-Azores) site from June 2009 through December 2010. Cloud properties derived from ARM ground-based observations were averaged over a 1 h interval centered at the satellite overpass time, while the CERES-MODIS (CM) results were averaged within a 30 km x 30 km grid box centered over the Azores site. A total of 63 daytime and 92 nighttime single-layered overcast MBL cloud cases were selected from 19 months of ARM radar-lidar and satellite observations. The CM cloud top/base heights (H-top/H-base) were determined from cloud top/base temperatures (T-top/T-base) using a regional boundary layer lapse rate method. For daytime comparisons, the CM-derived H-top (H-base), on average, is 0.063 km (0.068 km) higher (lower) than its ARM radar-lidar-observed counterpart, and the CM-derived T-top and T-base are 0.9 K less and 2.5 K greater than the surface values with high correlations (R-2 = 0.82 and 0.84, respectively). In general, the cloud top comparisons agree better than the cloud base comparisons, because the CM cloud base temperatures and heights are secondary products determined from cloud top temperatures and heights. No significant day-night difference was found in the analyses. The comparisons of MBL cloud microphysical properties reveal that when averaged over a 30 km x 30 km area, the CM-retrieved cloud droplet effective radius (r(e)) at 3.7 mu m is 1.3 mu m larger than that from the ARM retrievals (12.8 mu m), while the CM-retrieved cloud liquid water path (LWP) is 13.5 gm(-2) less than its ARM counterpart (114.2 gm(-2)) due to its small optical depth (9.6 versus 13.7). The differences are reduced by 50% when the CM averages are computed only using the MODIS pixel nearest the AMF site. Using the effective radius retrieved using 2.1 mu m channel to calculate LWP can reduce the difference between the CM and ARM microwave radiometer retrievals from -13.7 to 2.1 gm(-2). The 10% differences between the ARM and CERES-MODIS LWP and r(e) retrievals are within the uncertainties of the ARM LWP (similar to 20 gm(-2)) and r(e) (similar to 10%) retrievals; however, the 30% difference in optical depth is significant. Possible reasons contributing to this discrepancy are increased sensitivities in optical depth from both surface retrievals when tau similar to 10 and topography. The tau differences vary with wind direction and are consistent with the island orography. Much better agreement in tau is obtained when using only those data taken when the wind is from the northeast, where topographical effects on the sampled clouds are minimal.
C1 [Xi, Baike; Dong, Xiquan] Univ N Dakota, Dept Atmospher Sci, Grand Forks, ND 58201 USA.
[Minnis, Patrick] NASA, Langley Res Ctr, Hampton, VA 23665 USA.
[Sun-Mack, Sunny] SSAI, Hampton, VA USA.
RP Xi, BK (reprint author), Univ N Dakota, Dept Atmospher Sci, Grand Forks, ND 58201 USA.
EM baike@aero.und.edu
RI Minnis, Patrick/G-1902-2010;
OI Minnis, Patrick/0000-0002-4733-6148; Dong, Xiquan/0000-0002-3359-6117
FU U.S. Department of Energy (DOE) Office of Energy Research, Office of
Health and Environmental Research, Environmental Sciences Division; NASA
CERES project [NNX10AI05G]; DOE ASR project at University of North
Dakota [DE-SC008468]; DOE ASR project at NASA Langley Research Center
[DE-SC0000991]
FX The ground-based measurements were obtained from the Atmospheric
Radiation Measurement (ARM) Program sponsored by the U.S. Department of
Energy (DOE) Office of Energy Research, Office of Health and
Environmental Research, Environmental Sciences Division. The data can be
downloaded from http://www.archive.arm.gov/. The satellite data were
obtained from the NASA CERES cloud working group at the NASA Langley
Research Center. This research was supported by the NASA CERES project
under grant NNX10AI05G and DOE ASR project under grant DE-SC008468 at
University of North Dakota and DE-SC0000991 at the NASA Langley Research
Center. Dates and times corresponding to the sample numbers used in
several figures are available from the lead author on request.
NR 58
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U2 15
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 AUG 16
PY 2014
VL 119
IS 15
BP 9509
EP 9529
DI 10.1002/2014JD021813
PG 21
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA AO2ZK
UT WOS:000341197400020
ER
PT J
AU Warner, TA
Lang, TJ
Lyons, WA
AF Warner, Tom A.
Lang, Timothy J.
Lyons, Walter A.
TI Synoptic scale outbreak of self-initiated upward lightning (SIUL) from
tall structures during the central U. S. blizzard of 1-2 February 2011
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
ID LAKE-EFFECT THUNDERSTORMS; WINTER THUNDERSTORMS; UNITED-STATES;
DISCHARGES; SPRITES; EVENTS; STROKES; RADAR; COAST
AB A major central U. S. winter cyclone on 1-2 February 2011 produced a band of high winds, up to 75 cm of snow, and numerous reports of thundersnow from Oklahoma into Ontario over a 26 h period. The National Lightning Detection Network (NLDN) recorded 282 flashes comprised of 1153 events which were >96% negative polarity. Hopes of imaging winter sprites associated with energetic positive cloud-to-ground events that sometimes accompany such winter storms did not materialize. However, the lack of lightning over the Great Lakes waters, plus media reports of numerous thundersnow events in downtown Chicago, prompted a detailed analysis of the NLDN data. This revealed that >93% of all lightning in the snow band was likely or possibly associated with self-initiated upward lightning (SIUL) events from a variety of tall, and some not so tall, structures. In addition to 43 events from two Chicago skyscrapers, many shorter structures were involved, including wind turbines (13.1% of the total) and transmission line towers (6.7%). Wind speeds for all events exceeded the 8 m s(-1) minimum threshold associated with SIULs in Japanese winter lightning storms. Radar reflectivities at the event locations had a mean of 28 dBZ and were almost always <35 dBZ. While conventional radar displays suggested stratiform precipitation in the thundersnow region, detailed analysis of 3-D-gridded NMQ (National Mosaic and Multi-Sensor Quantitative Precipitation Estimation) radar reflectivity data confirmed elevated embedded cellular convection spanning the -10 degrees C region associated with isentropic lifting above a frontal surface, evidence of noninductive charge generation sufficient to allow upward leader initiation from tall objects.
C1 [Warner, Tom A.] ZTResearch, Rapid City, SD 57702 USA.
[Lang, Timothy J.] NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA.
[Lyons, Walter A.] FMA Res Inc, Ft Collins, CO USA.
RP Lyons, WA (reprint author), ZTResearch, Rapid City, SD 57702 USA.
EM walyons@frii.com
OI Lang, Timothy/0000-0003-1576-572X; Warner, Tom/0000-0001-8589-3351
FU Defense Advanced Research Projects Agency under the NIMBUS program;
National Science Foundation [AGS-1010657]; NSF [AGS-1048103]
FX Vaisala, Inc. graciously supplied the NLDN stroke-level data analyzed in
this study. The NLDN also enables the CMCN by providing geolocation of
high-iCMC strokes via a real-time, stroke-level data feed. The ongoing
efforts of Steven Cummer at Duke University to maintain and operate the
CMCN are vital to this and many related studies. The NMQ radar
reflectivity mosaics were provided by NOAA's National Severe Storms
Laboratory. The authors especially wish to thank Robert Rauber for his
valuable insights into the nature of embedded convection within the
comma cloud of winter cyclones. This research was partially supported by
awards from the Defense Advanced Research Projects Agency under the
NIMBUS program (to Duke University and NASA Marshall Space Flight
Center) and a National Science Foundation grant AGS-1010657 to Colorado
State University, and especially for the assistance of Steven Cummer and
Steven Rutledge. This research was also partially funded by NSF grant
AGS-1048103 to South Dakota School of Mines and Technology. We would
like to acknowledge and thank Alana Ballweber and Ryan Lueck from the
South Dakota School of Mines and Technology for providing data and
analysis from the 4 October 2013 Rapid City, SD, blizzard events. The
views, opinions, and findings in this report are those of the authors
and should not be construed as an official NASA or U.S. Government
position, policy, or decision. Data availability: Figure 1 was derived
from http://www.crh.noaa.gov/arx/?n=feb0211. NLDN data are available for
purchase from Vaisala, Inc., via
http://www.vaisala.com/en/products/thunderstormandlightningdetectionsyst
ems/Pages/NLDN.aspx. The tower database is available from
http://wireless.fcc.gov/antenna/index.htm?&job=home. Google Earth, used
for the identification of additional towers, is available from
http://www.google.com/earth/. Microsoft Office (used in the management
of the NLDN and tower databases as well as the composition of this
article) is available from http://office.microsoft.com. Satellite and
related weather imagery were obtained from
http://www.mmm.ucar.edu/imagearchive. National Charge Moment Change data
for this case are available upon request from Duke University
(cummer@ee.duke.edu). NMQ reflectivity mosaics may be obtained by
contacting NSSL (http://www.nssl.noaa.gov). Single NEXRAD radar data
were obtained from the National Climate Data Center
(http://www.ncdc.noaa.gov/). RUC data were pulled from
http://nomads.ncdc.noaa.gov/data/rucanl/201102/. The Interactive Data
Language (IDL) scripts used to analyze the data
NR 70
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U1 2
U2 17
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 AUG 16
PY 2014
VL 119
IS 15
BP 9530
EP 9548
DI 10.1002/2014JD021691
PG 19
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA AO2ZK
UT WOS:000341197400021
ER
PT J
AU Perez-Ramirez, D
Whiteman, DN
Smirnov, A
Lyamani, H
Holben, BN
Pinker, R
Andrade, M
Alados-Arboledas, L
AF Perez-Ramirez, Daniel
Whiteman, David N.
Smirnov, Alexander
Lyamani, Hassan
Holben, Brent N.
Pinker, Rachel
Andrade, Marcos
Alados-Arboledas, Lucas
TI Evaluation of AERONET precipitable water vapor versus microwave
radiometry, GPS, and radiosondes at ARM sites
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
ID GLOBAL POSITIONING SYSTEM; MOLECULAR SPECTROSCOPIC DATABASE; RADIATION
MEASUREMENT SITE; SPECTRAL-LINE DATABASE; ATMOSPHERIC RADIATION;
LOGNORMAL-DISTRIBUTION; OPTICAL-PROPERTIES; VAISALA RS92; RAMAN LIDAR;
DRY BIAS
AB In this paper we present comparisons of Aerosol Robotic Network (AERONET) precipitable water vapor (W) retrievals from Sun photometers versus radiosonde observations and other ground-based retrieval techniques such as microwave radiometry (MWR) and GPS. The comparisons make use of the extensive measurements made within the U.S. Department of Energy Atmospheric Radiation Measurement Program (ARM), mainly at their permanent sites located at the Southern Great Plains (Oklahoma, U.S.), Nauru Islands, and Barrow (Alaska, U.S.). These places experience different types of weather which allows the comparison of W under different conditions. Radiosonde and microwave radiometry data were provided by the ARM program while the GPS data were obtained from the SOUMINET network. In general, W obtained by AERONET is lower than those obtained by MWR and GPS by similar to 6.0-9.0% and similar to 6.0-8.0%, respectively. The AERONET values are also lower by approximately 5% than those obtained from the numerous balloon-borne radiosondes launched at the Southern Great Plains. These results point toward a consistent dry bias in the retrievals of W by AERONET of approximately 5-6% and a total estimated uncertainty of 12-15%. Differences with respect to MWR retrievals are a function of solar zenith angle pointing toward a possible bias in the MWR retrievals. Finally, the ability of AERONET precipitable water vapor retrievals to provide long-term records of W in diverse climate regimes is demonstrated.
C1 [Perez-Ramirez, Daniel; Whiteman, David N.] NASA, Goddard Space Flight Ctr, Mesoscale Atmospher Proc Lab, Greenbelt, MD 20771 USA.
[Perez-Ramirez, Daniel; Lyamani, Hassan; Alados-Arboledas, Lucas] Univ Granada, Dept Fis Aplicada, Granada, Spain.
[Perez-Ramirez, Daniel] Univ Space Res Assoc, Columbia, MD USA.
[Smirnov, Alexander; Holben, Brent N.] NASA, Goddard Space Flight Ctr, Biospher Sci Branch, Greenbelt, MD 20771 USA.
[Smirnov, Alexander] Sigma Space Corp, Lanham, MD USA.
[Lyamani, Hassan; Alados-Arboledas, Lucas] Andalusian Inst Earth Syst Res IISTA, Granada, Spain.
[Pinker, Rachel] Univ Maryland, Dept Atmospher & Ocean Sci, College Pk, MD 20742 USA.
[Andrade, Marcos] Univ Mayor de San Andres, Lab Atmospher Phys, La Paz, Bolivia.
RP Perez-Ramirez, D (reprint author), NASA, Goddard Space Flight Ctr, Mesoscale Atmospher Proc Lab, Greenbelt, MD 20771 USA.
EM daniel.perezramirez@nasa.gov
RI Alados-Arboledas, Lucas/P-5630-2014; Pinker, Rachel/F-6565-2010;
Perez-Ramirez, Daniel/Q-1129-2016; Smirnov, Alexander/C-2121-2009;
OI Alados-Arboledas, Lucas/0000-0003-3576-7167; Perez-Ramirez,
Daniel/0000-0002-7679-6135; Smirnov, Alexander/0000-0002-8208-1304;
Lyamani, Hassan/0000-0002-6386-1102
FU NASA/Goddard Space Flight Center; Spanish Ministry of Science and
Technology [CGL2010-18782, CSD2007-00067]; Andalusian Regional
Government [P10-RNM-6299, P08-RNM-3568]; EU through ACTRIS project [EU
INFRA-2010-1.1.16-262254]; Postdoctoral Program of the University of
Granada
FX The data of AERONET Sun photometry used here are available at
http://aeronet.gsfc.nasa.gov/. Radiosondes and microwave radiometers
data are available in ARM data archive at
http://www.archive.arm.gov/armlogin/login.jsp. Finally, GPS data used
are available through SOUMINET webpage at
http://www.suominet.ucar.edu/data/index.html. We thank ARM program for
providing microwave radiometry and radiosonde data. We also are thankful
to SOUMINET network for providing GPS data. This work was supported by
NASA/Goddard Space Flight Center, by the Spanish Ministry of Science and
Technology through projects CGL2010-18782 and CSD2007-00067, by the
Andalusian Regional Government through projects P10-RNM-6299 and
P08-RNM-3568, by EU through ACTRIS project (EU
INFRA-2010-1.1.16-262254), and by the Postdoctoral Program of the
University of Granada.
NR 72
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U2 15
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 AUG 16
PY 2014
VL 119
IS 15
BP 9596
EP 9613
DI 10.1002/2014JD021730
PG 18
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA AO2ZK
UT WOS:000341197400025
ER
PT J
AU Baek, KH
Kim, JH
Park, RJ
Chance, K
Kurosu, TP
AF Baek, K. H.
Kim, Jae H.
Park, Rokjin J.
Chance, Kelly
Kurosu, Thomas P.
TI Validation of OMI HCHO data and its analysis over Asia
SO SCIENCE OF THE TOTAL ENVIRONMENT
LA English
DT Article
DE OMI HCHO; EOF; SVD; Megacity pollution; Biomass burning
ID ISOPRENE EMISSIONS; SATELLITE-OBSERVATIONS; COLUMN OBSERVATIONS;
NORTH-AMERICA; FORMALDEHYDE; VARIABILITY; SPACE; AIR; OZONE; CHEMISTRY
AB OMI HCHO is validated over the continental US (CONUS), and used to analyze regional sources in Northeast Asia (NA) and Southeast Asia (SA). OMI HCHO Version 2.0 data show unrealistic trends, which prompted the production of a corrected OMI HCHO data set. EOF and SVD are utilized to compare the spatial and temporal variability between OMI HCHO against GOME and SCIAMACHY, and against GEOS-Chem. CONUS HCHO chemistry is well studied; its concentrations are greatest in the southeastern US with annual cycle maximums corresponding to the summer vegetation. The corrected OMI HCHO agrees with this understanding as well as with the other sensors measurements and has no unrealistic trends. In NA the annual cycle is super-posed by extremely large concentrations in polluted mega-cities. The other sensors generally agree with NA's OMI HCHO regional distribution, but megacity signal is not seen in GEOS-Chem. Our study supports the findings proposed by others that the emission inventory used in GEOS-Chem significantly underestimates anthropogenic influence on HCHO emission over megacities. The persistent mega-city signal is also present in SA. In SA the spatial and temporal patterns of OMI HCHO show a maximum in the dry season. The patterns are in remarkably good agreement with fire counts, which illustrates that the variability of HCHO over SA is strongly influenced by biomass burning. The corrected OMI HCHO data has realistic trends, conforms to well-known sources over CONUS, and has shown a stationary large concentration over polluted Asian mega-cities, and a widespread biomass burning in SA. (C) 2014 Elsevier B.V. All rights reserved.
C1 [Baek, K. H.; Kim, Jae H.] Pusan Natl Univ, Dept Atmospher Sci, Pusan, South Korea.
[Park, Rokjin J.] Seoul Natl Univ, Sch Earth & Environm Sci, Seoul, South Korea.
[Chance, Kelly] Harvard Smithsonian Ctr Astrophys, Cambridge, MA USA.
[Kurosu, Thomas P.] CA Inst Technol, Jet Prop Lab, Pasadena, CA USA.
RP Kim, JH (reprint author), Pusan Natl Univ, Dept Atoms Sci, Room 525-1, Pusan, South Korea.
EM jaekim@pusan.ac.kr
RI Chem, GEOS/C-5595-2014; Park, Rokjin/I-5055-2012;
OI Park, Rokjin/0000-0001-8922-0234; Chance, Kelly/0000-0002-7339-7577
FU National Research Foundation of Korea (NRF) - Ministry of Education,
Science and Technology [2012R1A1A2040757]
FX This research was supported by the Basic Science Research Program
through the National Research Foundation of Korea (NRF) funded by the
Ministry of Education, Science and Technology (2012R1A1A2040757).
NR 44
TC 0
Z9 0
U1 2
U2 19
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0048-9697
EI 1879-1026
J9 SCI TOTAL ENVIRON
JI Sci. Total Environ.
PD AUG 15
PY 2014
VL 490
BP 93
EP 105
DI 10.1016/j.scitotenv.2014.04.108
PG 13
WC Environmental Sciences
SC Environmental Sciences & Ecology
GA AY0NT
UT WOS:000347293800011
PM 24840284
ER
PT J
AU Dietrich, JP
Van Gaest, AL
Strickland, SA
Hutchinson, GP
Krupkin, AB
Arkoosh, MR
AF Dietrich, Joseph P.
Van Gaest, Ahna L.
Strickland, Stacy A.
Hutchinson, Greg P.
Krupkin, Alex B.
Arkoosh, Mary R.
TI Toxicity of PHOS-CHEK LC-95A and 259F fire retardants to ocean- and
stream-type Chinook salmon and their potential to recover before
seawater entry
SO SCIENCE OF THE TOTAL ENVIRONMENT
LA English
DT Article
DE Salmon; Wildfire; Toxicity; PHOS-CHEK; Smoltification; Fire retardant
ID TROUT ONCORHYNCHUS-MYKISS; EARLY-LIFE STAGES; RAINBOW-TROUT; SMOLT
TRANSFORMATION; CHEMICALS; AMMONIA; PARR; EXPOSURE; SMOLTIFICATION;
TSHAWYTSCHA
AB Long-termfire retardants are used to prevent the spread ofwildland fire, but have inadvertently entered aquatic habitats and resulted in fish kills. Weexamined the toxicity of two fire retardant products; PHOS-CHEK 259F and LC-95A, on Chinook salmon with two different life histories, ocean-type and stream-type, at different stages of their development. Ocean-type Chinook outmigrate to the ocean as subyearlings; while, stream-type salmon overwinter in freshwater and outmigrate as yearlings. Ocean-type and stream-type salmon were exposed to the fire retardants prior to their parr to smolt transition (presmolts) as subyearlings (stream-type and oceantype) and yearlings (stream-type only), as well as during their transition (smolts). The salmon were exposed to eight concentrations of each retardant and a control for 96 h to determine acute toxicity. Lethal concentration curves were modeled by logistic regression for each life history and life stage exposed to the two fire retardants. Among all life histories and life stages tested, PHOS-CHEK 259F was most toxic to stream-type salmon at smolt stage and PHOS-CHEK LC-95A was most toxic to ocean-type salmon at smolt stage. To determine the delayed effects of product exposures on fish health as well as for the potential of recovery, 24-hour seawater challenges were performed immediately after fire retardant exposure, as well as after a recovery period. Previous PHOSCHEK exposure reduced survival during seawater challenge among salmon from both life histories undergoing the parr-smolt transition and was more pronounced after PHOS-CHEK LC-95A exposure. However, this delayed effect was not observed 34 or more days after either PHOS-CHEK exposure. We conclude that accidental PHOSCHEK LC-95A or 259F drops during salmon outmigration would have adverse impacts that extend beyond the acute mortality that occurs within the immediate drop and dilution areas. Published by Elsevier B.V.
C1 [Dietrich, Joseph P.; Van Gaest, Ahna L.; Strickland, Stacy A.; Hutchinson, Greg P.; Krupkin, Alex B.; Arkoosh, Mary R.] NOAA, Environm & Fisheries Sci Div, NW Fisheries Sci Ctr, Natl Marine Fisheries Serv, Newport, OR 97365 USA.
RP Dietrich, JP (reprint author), 2032 SE OSU Dr, Newport, OR 97365 USA.
EM joseph.dietrich@noaa.gov; vangaest@gmail.com; sas70@me.com;
hutching@onid.orst.edu; krupkinalex@gmail.com; mary.arkoosh@noaa.gov
FU U.S. Department of Agriculture-Forest Service Wildland Fire Chemical
Systems Program [10-IA-11130206-046]
FX We are sincerely grateful for the technical efforts of Deborah Boylen
and the animal care assistance provided by Kalle Applegate, Lauren
Arkoosh, Stacie Farwell, Athena Jackson, and Alice McKinstry. We also
appreciate the insights provided by Edward E. Little, U.S. Geological
Survey-CERC, Columbia, Missouri. The present study was financially
supported by the U.S. Department of Agriculture (#
10-IA-11130206-046)-Forest Service Wildland Fire Chemical Systems
Program.
NR 37
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U1 5
U2 16
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0048-9697
EI 1879-1026
J9 SCI TOTAL ENVIRON
JI Sci. Total Environ.
PD AUG 15
PY 2014
VL 490
BP 610
EP 621
DI 10.1016/j.scitotenv.2014.05.038
PG 12
WC Environmental Sciences
SC Environmental Sciences & Ecology
GA AY0NT
UT WOS:000347293800065
PM 24880550
ER
PT J
AU Robertson, FR
Bosilovich, MG
Roberts, JB
Reichle, RH
Adler, R
Ricciardulli, L
Berg, W
Huffman, GJ
AF Robertson, F. R.
Bosilovich, M. G.
Roberts, J. B.
Reichle, R. H.
Adler, R.
Ricciardulli, L.
Berg, W.
Huffman, G. J.
TI Consistency of Estimated Global Water Cycle Variations over the
Satellite Era
SO JOURNAL OF CLIMATE
LA English
DT Article
ID PACIFIC DECADAL VARIABILITY; CLIMATOLOGY PROJECT GPCP; DATA ASSIMILATION
SYSTEM; SEA-SURFACE TEMPERATURE; LAND-SURFACE; PRECIPITATION PATTERNS;
ATMOSPHERIC MOISTURE; HYDROLOGICAL CYCLE; HEAT FLUXES; WIND-SPEED
AB Motivated by the question of whether recent interannual to decadal climate variability and a possible "climate shift" may have affected the global water balance, we examine precipitation minus evaporation (P - E) variability integrated over the global oceans and global land for the period 1979-2010 from three points of view-remotely sensed retrievals and syntheses over the oceans, reanalysis vertically integrated moisture flux convergence (VMFC) over land, and land surface models (LSMs) forced with observations-based precipitation, radiation, and near-surface meteorology.
Over land, reanalysis VMFC and P - evapotranspiration (ET) from observationally forced LSMs agree on interannual variations (e.g., El Nino/La Nina events); however, reanalyses exhibit upward VMFC trends 3-4 times larger than P - ET trends of the LSMs. Experiments with other reanalyses using reduced observations show that upward VMFC trends in the full reanalyses are due largely to observing system changes interacting with assimilation model physics. The much smaller P - ET trend in the LSMs appears due to changes in frequency and amplitude of warm events after the 1997/98 El Nino, a result consistent with coolness in the eastern tropical Pacific sea surface temperature (SST) after that date.
When integrated over the global oceans, E and especially P variations show consistent signals of El Nino/La Nina events. However, at scales longer than interannual there is considerable uncertainty especially in E. This results from differences among datasets in near-surface atmospheric specific humidity and wind speed used in bulk aerodynamic retrievals. The P variations, all relying substantially on passive microwave retrievals over ocean, also have uncertainties in decadal variability, but to a smaller degree.
C1 [Robertson, F. R.; Roberts, J. B.] NASA, Earth Sci Off, Marshall Space Flight Ctr, Huntsville, AL 35805 USA.
[Bosilovich, M. G.; Reichle, R. H.] NASA, Goddard Space Flight Ctr, Global Modeling & Assimilat Off, Greenbelt, MD 20771 USA.
[Adler, R.] Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20742 USA.
[Ricciardulli, L.] Remote Sensing Syst, Santa Rosa, CA USA.
[Berg, W.] Colorado State Univ, Dept Atmospher Sci, Ft Collins, CO 80523 USA.
[Huffman, G. J.] NASA, Goddard Space Flight Ctr, Mesoscale Atmospher Proc Lab, Greenbelt, MD 20771 USA.
RP Robertson, FR (reprint author), NASA, Earth Sci Off, Marshall Space Flight Ctr, 320 Sparkman Dr, Huntsville, AL 35805 USA.
EM pete.robertson@nasa.gov
RI Reichle, Rolf/E-1419-2012; Huffman, George/F-4494-2014; Bosilovich,
Michael/F-8175-2012
OI Huffman, George/0000-0003-3858-8308;
FU NASA Energy and Water Cycle Study (NEWS)
FX The NASA Energy and Water Cycle Study (NEWS), Dr. Jared Entin, program
manager, provided funding for this work. NEWS has been instrumental in
encouraging cross-collaborative interactions both internal and external
to the investigator team. The authors gratefully acknowledge discussions
with numerous individuals, both data providers and users, whose
suggestions and clarifications have added substantially to the paper.
These include Chung-Lin Shie and Matt Rodell, NASA Goddard Space Flight
Center; Lisan Yu and Carol Anne Clayson, Woods Hole Oceanographic
Institution; Carl Mears and Kyle Hilburn of Remote Sensing Systems,
Inc.; and Martin Jung and Markus Reichstein, Max Plank Institute for
Biogeochemistry. The comments of three anonymous reviewers added
significantly to this manuscript.
NR 90
TC 8
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U1 0
U2 20
PU AMER METEOROLOGICAL SOC
PI BOSTON
PA 45 BEACON ST, BOSTON, MA 02108-3693 USA
SN 0894-8755
EI 1520-0442
J9 J CLIMATE
JI J. Clim.
PD AUG 15
PY 2014
VL 27
IS 16
BP 6135
EP 6154
DI 10.1175/JCLI-D-13-00384.1
PG 20
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA AN0YV
UT WOS:000340310800003
ER
PT J
AU Westphal, AJ
Stroud, RM
Bechtel, HA
Brenker, FE
Butterworth, AL
Flynn, GJ
Frank, DR
Gainsforth, Z
Hillier, JK
Postberg, F
Simionovici, AS
Sterken, VJ
Nittler, LR
Allen, C
Anderson, D
Ansari, A
Bajt, S
Bastien, RK
Bassim, N
Bridges, J
Brownlee, DE
Burchell, M
Burghammer, M
Changela, H
Cloetens, P
Davis, AM
Doll, R
Floss, C
Gruen, E
Heck, PR
Hoppe, P
Hudson, B
Huth, J
Kearsley, A
King, AJ
Lai, B
Leitner, J
Lemelle, L
Leonard, A
Leroux, H
Lettieri, R
Marchant, W
Ogliore, R
Ong, WJ
Price, MC
Sandford, SA
Tresseras, JAS
Schmitz, S
Schoonjans, T
Schreiber, K
Silversmit, G
Sole, VA
Srama, R
Stadermann, F
Stephan, T
Stodolna, J
Sutton, S
Trieloff, M
Tsou, P
Tyliszczak, T
Vekemans, B
Vincze, L
Von Korff, J
Wordsworth, N
Zevin, D
Zolensky, ME
AF Westphal, Andrew J.
Stroud, Rhonda M.
Bechtel, Hans A.
Brenker, Frank E.
Butterworth, Anna L.
Flynn, George J.
Frank, David R.
Gainsforth, Zack
Hillier, Jon K.
Postberg, Frank
Simionovici, Alexandre S.
Sterken, Veerle J.
Nittler, Larry R.
Allen, Carlton
Anderson, David
Ansari, Asna
Bajt, Sasa
Bastien, Ron K.
Bassim, Nabil
Bridges, John
Brownlee, Donald E.
Burchell, Mark
Burghammer, Manfred
Changela, Hitesh
Cloetens, Peter
Davis, Andrew M.
Doll, Ryan
Floss, Christine
Gruen, Eberhard
Heck, Philipp R.
Hoppe, Peter
Hudson, Bruce
Huth, Joachim
Kearsley, Anton
King, Ashley J.
Lai, Barry
Leitner, Jan
Lemelle, Laurence
Leonard, Ariel
Leroux, Hugues
Lettieri, Robert
Marchant, William
Ogliore, Ryan
Ong, Wei Jia
Price, Mark C.
Sandford, Scott A.
Tresseras, Juan-Angel Sans
Schmitz, Sylvia
Schoonjans, Tom
Schreiber, Kate
Silversmit, Geert
Sole, Vicente A.
Srama, Ralf
Stadermann, Frank
Stephan, Thomas
Stodolna, Julien
Sutton, Stephen
Trieloff, Mario
Tsou, Peter
Tyliszczak, Tolek
Vekemans, Bart
Vincze, Laszlo
Von Korff, Joshua
Wordsworth, Naomi
Zevin, Daniel
Zolensky, Michael E.
CA 30714 Stardust Home Dusters
TI Evidence for interstellar origin of seven dust particles collected by
the Stardust spacecraft
SO SCIENCE
LA English
DT Article
ID COMET 81P/WILD 2; SOLAR-SYSTEM; INTERPLANETARY DUST; SIZE DISTRIBUTION;
GRAINS; IMPACTS; AEROGEL; EVENTS; WILD-2; RETURN
AB Seven particles captured by the Stardust Interstellar Dust Collector and returned to Earth for laboratory analysis have features consistent with an origin in the contemporary interstellar dust stream. More than 50 spacecraft debris particles were also identified. The interstellar dust candidates are readily distinguished from debris impacts on the basis of elemental composition and/or impact trajectory. The seven candidate interstellar particles are diverse in elemental composition, crystal structure, and size. The presence of crystalline grains and multiple iron-bearing phases, including sulfide, in some particles indicates that individual interstellar particles diverge from any one representative model of interstellar dust inferred from astronomical observations and theory.
C1 [Westphal, Andrew J.; Butterworth, Anna L.; Gainsforth, Zack; Anderson, David; Lettieri, Robert; Marchant, William; Stodolna, Julien; Von Korff, Joshua; Zevin, Daniel] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
[Stroud, Rhonda M.; Bassim, Nabil] Naval Res Lab, Mat Sci & Technol Div, Washington, DC USA.
[Bechtel, Hans A.; Tyliszczak, Tolek] Lawrence Berkeley Lab, Adv Light Source, Berkeley, CA USA.
[Brenker, Frank E.; Schmitz, Sylvia] Goethe Univ Frankfurt, Geosci Inst, D-60054 Frankfurt, Germany.
[Flynn, George J.] SUNY Coll Plattsburgh, Plattsburgh, NY 12901 USA.
[Frank, David R.; Bastien, Ron K.] NASA Johnson Space Ctr JSC, Jacobs Technol ESCG, Houston, TX USA.
[Hillier, Jon K.; Postberg, Frank; Trieloff, Mario] Heidelberg Univ, Inst Geowissensch, D-69115 Heidelberg, Germany.
[Simionovici, Alexandre S.] Observ Sci Univers Grenoble, Inst Sci Terre, Grenoble, France.
[Sterken, Veerle J.] Univ Stuttgart, Inst Raumfahrtsyst IRS, D-70174 Stuttgart, Germany.
[Sterken, Veerle J.] TU Braunschweig, IGEP, Braunschweig, Germany.
[Sterken, Veerle J.; Gruen, Eberhard] Max Planck Inst Kernphys, D-69117 Heidelberg, Germany.
[Sterken, Veerle J.; Heck, Philipp R.] Int Space Sci Inst, Bern, Switzerland.
[Nittler, Larry R.] Carnegie Inst Sci, Washington, DC USA.
[Allen, Carlton; Zolensky, Michael E.] NASA JSC, Houston, TX USA.
[Ansari, Asna] Field Museum Nat Hist, Chicago, IL 60605 USA.
[Bajt, Sasa] DESY, Hamburg, Germany.
[Bridges, John] Univ Leicester, Space Res Ctr, Leicester, Leics, England.
[Brownlee, Donald E.] Univ Washington, Dept Astron, Seattle, WA 98195 USA.
[Burchell, Mark; Price, Mark C.] Univ Kent, Canterbury, Kent, England.
[Burghammer, Manfred; Schoonjans, Tom; Silversmit, Geert; Vekemans, Bart; Vincze, Laszlo] Univ Ghent, B-9000 Ghent, Belgium.
[Changela, Hitesh] Univ New Mexico, Albuquerque, NM 87131 USA.
[Cloetens, Peter; Tresseras, Juan-Angel Sans; Sole, Vicente A.] ESRF, Grenoble, France.
[Davis, Andrew M.; King, Ashley J.; Stephan, Thomas] Univ Chicago, Chicago, IL 60637 USA.
[Doll, Ryan; Floss, Christine; Leonard, Ariel; Ong, Wei Jia; Schreiber, Kate; Stadermann, Frank] Washington Univ, St Louis, MO USA.
[Hoppe, Peter; Huth, Joachim; Leitner, Jan] Max Planck Inst Chem, D-55128 Mainz, Germany.
[Kearsley, Anton] Nat Hist Museum, London SW7 5BD, England.
[Lai, Barry; Sutton, Stephen] Argonne Natl Lab, Adv Photon Source, Lemont, IL USA.
[Lemelle, Laurence] Ecole Normale Super Lyon, F-69364 Lyon, France.
[Leroux, Hugues] Univ Lille 1, F-59655 Villeneuve Dascq, France.
[Ogliore, Ryan] Univ Hawaii Manoa, Honolulu, HI 96822 USA.
[Sandford, Scott A.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Srama, Ralf] Univ Stuttgart, IRS, D-70174 Stuttgart, Germany.
[Tsou, Peter] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Wordsworth, Naomi] Wexbury, Stoke Poges, Bucks, England.
RP Westphal, AJ (reprint author), Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
EM westphal@ssl.berkeley.edu
RI Sans Tresserras, Juan Angel/J-9362-2014; Leitner, Jan/A-7391-2015;
Hoppe, Peter/B-3032-2015; Bajt, Sasa/G-2228-2010; Stroud,
Rhonda/C-5503-2008;
OI Sans Tresserras, Juan Angel/0000-0001-9047-3992; Leitner,
Jan/0000-0003-3655-6273; Hoppe, Peter/0000-0003-3681-050X; Stroud,
Rhonda/0000-0001-5242-8015; Burchell, Mark/0000-0002-2680-8943
FU NASA [NNX09AC36G, NNX09AC63G, NNH11AQ61I, NNX11AC21G, NNX11AE15G];
Office of Science, Office of Basic Energy Sciences, of the U.S.
Department of Energy (DOE) [DE-AC02-05CH11231]; U.S. DOE, Office of
Science, Office of Basic Energy Sciences [DE-AC02-98CH10886]; U.S. DOE
[DE-AC02-06CH11357]; Klaus Tschira foundation; Tawani Foundation;
Science and Technology Facilities Council (UK); German Science
Foundation (DFG) [SPP1385]; Funds for Scientific Research (FWO),
Flanders, Belgium [G.0395.11, G.0257.12N, G.0C12.13]
FX We are deeply grateful to the Stardust@home dusters (list at
http://stardustathome.ssl.berkeley.edu/sciencedusters), whose tremendous
efforts were critically important to the success of this project. The
ISPE consortium gratefully acknowledges the NASA Discovery Program for
Stardust, the fourth NASA Discovery mission. NASA grants supported the
following authors: NNX09AC36G-A.J.W., A. L. B., Z.G., R. L., D.Z., W.
M., and J.V.K.; NNX09AC63G-C.F., R. D., A. L., W.J.O., K. S., and
F.J.S.; NNH11AQ61I-R.M.S., H. C. G., and N.D.B.; NNX11AC21G-A.M.D.,
A.J.K., and T. S.; NNX11AE15G-G.J.F. The Advanced Light Source and the
National Center for Electron Microscopy are supported by the Director,
Office of Science, Office of Basic Energy Sciences, of the U.S.
Department of Energy (DOE) under contract no. DE-AC02-05CH11231. Use of
the National Synchrotron Light Source, Brookhaven National Laboratory,
was supported by the U.S. DOE, Office of Science, Office of Basic Energy
Sciences, under contract no. DE-AC02-98CH10886. Use of the Advanced
Photon Source, an Office of Science User Facility operated for the U. S.
DOE Office of Science by Argonne National Laboratory, was supported by
the U.S. DOE under contract no. DE-AC02-06CH11357. M. T. and F. P.
acknowledge support by Klaus Tschira foundation. A. A. and P. R. H. were
supported by the Tawani Foundation. M.J.B. and M. C. P. are supported by
Science and Technology Facilities Council (UK). F. E. B., J.K.H., P. H.,
J.L., F. P., S. S., R. S., and M. T. were supported by funding of the
German Science Foundation (DFG) within SPP1385: the first ten million
years of the solar system-a planetary materials approach. The ESRF ID13
measurements were performed in the framework of ESRF LTP EC337, with
financial support by the Funds for Scientific Research (FWO), Flanders,
Belgium (contract nr. G.0395.11, G.0257.12N and Big Science program
G.0C12.13). G. Silversmit was postdoctoral fellow of the FWO during the
ISPE investigations. Data presented in this paper are described in the
supplementary materials and in references (9-20).
NR 43
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U1 5
U2 67
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 AUG 15
PY 2014
VL 345
IS 6198
BP 786
EP 791
DI 10.1126/science.1252496
PG 6
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA AN4XM
UT WOS:000340593100038
PM 25124433
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 An experimental study of lunar dust erosive wear potential using the
JSC-1AF lunar dust simulant
SO WEAR
LA English
DT Article
DE Erosive wear; Lunar dust; Optical performance; Particle advection
ID SHAPE
AB The exhaust plumes from spacecraft landing on Earth's moon advect lunar dust particles which have been shown to erode, or "sandblast", nearby objects. Evidence of this phenomenon was provided by NASA's Apollo 12 mission during which exhaust ejecta, generated by the Apollo Lunar Module landing, erosively wore components of the Surveyor III lunar probe located 155 m from the Apollo 12 landing site. Recently, interest in new lunar missions has been expressed by a number of different groups including countries and private companies. With the potential for a large number of new lunar landings in relatively close proximity to each other and existing lunar hardware, efforts must be taken to understand the damage that lunar dust particle erosion can cause to material surfaces. In this work, a study was conducted with the JSC-1AF lunar dust simulant to understand the erosive potential of lunar dust. Metallic and acrylic test specimens were exposed to erosive wear and the changes in mass, surface topography, transmittance, and reflectance are reported. It was observed that exposure to erosive wear from JSC-1AF, even at moderate velocities (approximately 105 m/s), resulted in a significant decrease in direct transmittance and total reflectance greater than 70% in some cases. The results in this study suggest that optical components, such as lenses and mirrors are highly susceptible to damage during lunar landings due to lunar dust particle impingement. (C) 2014 Elsevier B.V. All rights reserved.
C1 [Mpagazehe, Jeremiah N.; Higgs, C. Fred, III] Carnegie Mellon Univ, Pittsburgh, PA 15213 USA.
[Street, Kenneth W., Jr.; Delgado, Irebert R.] NASA Glenn Res Ctr, Cleveland, OH 44135 USA.
RP Higgs, CF (reprint author), Carnegie Mellon Univ, 5000 Forbes Ave, Pittsburgh, PA 15213 USA.
EM higgs@andrew.cmu.edu
FU NASA Graduate Student Researchers (GSRP) Grant [NNX09AK96H]; Alfred P.
Sloan Foundation
FX The research in this work was supported by the NASA Graduate Student
Researchers (GSRP) Grant (NNX09AK96H). Additional funding for this work
was supplied by the Alfred P. Sloan Foundation. The authors are very
grateful to Jim Gaier (NASA Glenn Research Center) for his consultation
during the preparation of this manuscript. We also sincerely thank
Philip Metzger (NASA Kennedy Space Center) for helpful and insightful
discussions regarding this research. The authors would also like to
gratefully acknowledge, Richard Mondry Jr. (Gilcrest Electric and Supply
Co.) for his help constructing the experimental rig on which the tests
were performed. We are sincerely grateful to Michelle Mrdenovich (Sierra
Lobo Inc.), Laura Evans (NASA Glenn Research Center), and Joy Buehler
(Vantage Partners, LLC) for their substantial assistance with SEM
imaging, EDX analysis, and sample preparation.
NR 24
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U1 3
U2 7
PU ELSEVIER SCIENCE SA
PI LAUSANNE
PA PO BOX 564, 1001 LAUSANNE, SWITZERLAND
SN 0043-1648
J9 WEAR
JI Wear
PD AUG 15
PY 2014
VL 316
IS 1-2
BP 79
EP 91
DI 10.1016/j.wear.2014.04.018
PG 13
WC Engineering, Mechanical; Materials Science, Multidisciplinary
SC Engineering; Materials Science
GA AK7JX
UT WOS:000338605700009
ER
PT J
AU Dynys, FW
Sayir, A
Mackey, J
Sehirlioglu, A
AF Dynys, F. W.
Sayir, A.
Mackey, J.
Sehirlioglu, A.
TI Thermoelectric properties of WSi2-SixGe1-x composites
SO JOURNAL OF ALLOYS AND COMPOUNDS
LA English
DT Article
DE Thermoelectric materials; Microstructure; Crystal growth; Composite
materials; Electrical transport
ID GE-SI ALLOYS; THERMAL CONDUCTIVITY; DIRECTIONAL SOLIDIFICATION; HIGH
TEMPERATURES; SOLID-SOLUTIONS; FLASH METHOD; SILICIDE; DIFFUSIVITY;
NUCLEATION; GROWTH
AB Thermoelectric properties of the W/Si/Ge alloy system have been investigated with varying concentration levels of germanium and tungsten. The alloys were fabricated by directional solidification with the Bridgman method using boron nitride and fused silica crucibles. The effect of crucible contamination was investigated and found to result in doping the system to suitable levels for thermoelectric applications. The system has been demonstrated as a suitable high temperature p-type thermoelectric material exhibiting high power factors, >3000 mu W/m K-2. Seebeck coefficients of the system are on the order of +300 mu V/K and electrical conductivities of 2.8 x 10(4) S/m at the optimum operating temperature. The best composition, 0.9 at% W/9.3 at% Ge, achieved a figure of merit comparable to RTG values over the temperature range of interest. The results suggest that W addition can reduce the use of expensive Ge component of the alloy. Reported are the details of processing conditions, microstructure development, and temperature dependent thermoelectric properties. The material system was stable at the temperatures required for NASA's radioisotope thermoelectric generators. (C) 2014 Elsevier B.V. All rights reserved.
C1 [Dynys, F. W.; Sayir, A.] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA.
[Mackey, J.] Univ Akron, Dept Mech Engn, Akron, OH 44325 USA.
[Sehirlioglu, A.] Case Western Reserve Univ, Dept Mat Sci & Engn, Cleveland, OH 44106 USA.
RP Mackey, J (reprint author), Univ Akron, Dept Mech Engn, Akron, OH 44325 USA.
EM jam151@zips.uakron.edu
OI Mackey, Jonathan/0000-0003-1053-7007
FU NASA [NNX08AB43A]; AFOSR [FA9550-09-1-0312]
FX The work was funded through NASA cooperative agreement NNX08AB43A. Alp
Sehirlioglu acknowledges AFOSR FA9550-09-1-0312. The authors would like
to thank Thomas Sabo and Raymond Babuder for their assistance with the
experimental portion of the work.
NR 38
TC 8
Z9 8
U1 1
U2 60
PU ELSEVIER SCIENCE SA
PI LAUSANNE
PA PO BOX 564, 1001 LAUSANNE, SWITZERLAND
SN 0925-8388
EI 1873-4669
J9 J ALLOY COMPD
JI J. Alloy. Compd.
PD AUG 15
PY 2014
VL 604
BP 196
EP 203
DI 10.1016/j.jallcom.2014.03.133
PG 8
WC Chemistry, Physical; Materials Science, Multidisciplinary; Metallurgy &
Metallurgical Engineering
SC Chemistry; Materials Science; Metallurgy & Metallurgical Engineering
GA AG6CH
UT WOS:000335505600029
ER
PT J
AU Gandhiraman, RP
Nordlund, D
Javier, C
Koehne, JE
Chen, B
Meyyappan, M
AF Gandhiraman, Ram P.
Nordlund, Dennis
Javier, Cristina
Koehne, Jessica E.
Chen, Bin
Meyyappan, M.
TI X-ray Absorption Study of Graphene Oxide and Transition Metal Oxide
Nanocomposites
SO JOURNAL OF PHYSICAL CHEMISTRY C
LA English
DT Article
ID INNER-SHELL EXCITATION; FINE-STRUCTURE SPECTRA; LITHIUM ION BATTERIES;
ELECTROPHORETIC DEPOSITION; ELECTROCHEMICAL CAPACITORS; SUPERCAPACITOR
ELECTRODES; THIN-FILM; SPECTROSCOPY; ENERGY; PERFORMANCE
AB The surface properties of the electrode materials play a crucial role in determining the performance and efficiency of energy storage devices. Graphene oxide and nanostructures of 3d transition metal oxides were synthesized for construction of electrodes in supercapacitors, and the electronic structure and oxidation states were probed using near-edge X-ray absorption fine structure. Understanding the chemistry of graphene oxide would provide valuable insight into its reactivity and properties as the graphene oxide transformation to reduced-graphene oxide is a key step in the synthesis of the electrode materials. Polarized behavior of the synchrotron X-rays and the angular dependency of the near-edge X-ray absorption fine structures (NEXAFS) have been utilized to study the orientation of the sigma and pi bonds of the graphene oxide and graphene oxide-metal oxide nanocomposites. The core-level transitions of individual metal oxides and that of the graphene oxide nanocomposite showed that the interaction of graphene oxide with the metal oxide nanostructures has not altered the electronic structure of either of them. As the restoration of the pi network is important for good electrical conductivity, the C K edge NEXAFS spectra of reduced graphene oxide nanocomposites confirms the same through increased intensity of the sp(2)-derived unoccupied states pi* band. A pronounced angular dependency of the reduced sample and the formation of excitonic peaks confirmed the formation of extended conjugated network.
C1 [Gandhiraman, Ram P.; Javier, Cristina; Koehne, Jessica E.; Chen, Bin; Meyyappan, M.] NASA, Ames Res Ctr, Mountain View, CA 94035 USA.
[Nordlund, Dennis] Stanford Linear Accelerator Ctr, Stanford Synchrotron Radiat Lightsource, Menlo Pk, CA 94025 USA.
RP Gandhiraman, RP (reprint author), NASA, Ames Res Ctr, Mountain View, CA 94035 USA.
EM ramprasad.gandhiraman@nasa.gov
RI Gandhiraman, Ram Prasad/B-7004-2013; Nordlund, Dennis/A-8902-2008
OI Gandhiraman, Ram Prasad/0000-0001-8957-7938; Nordlund,
Dennis/0000-0001-9524-6908
FU U.S. Department of Energy, Office of Science, Office of Basic Energy
Sciences [DE-AC02-76SF00515]; DOE Office of Biological and Environmental
Research; National Institutes of Health, National Institute of General
Medical Sciences [P41GM103393]
FX R.P.G. is with Universities Space Research Association subcontracted to
NASA Ames Research Center under NASA cooperative agreement. The beam
time for synchrotron measurements was awarded to the authors through the
peer-reviewed SLAC research proposal No. 2163. Use of the Stanford
Synchrotron Radiation Lightsource, SLAC National Accelerator Laboratory,
is supported by the U.S. Department of Energy, Office of Science, Office
of Basic Energy Sciences under Contract No. DE-AC02-76SF00515. The SSRL
Structural Molecular Biology Program is supported by the DOE Office of
Biological and Environmental Research and by the National Institutes of
Health, National Institute of General Medical Sciences (including
P41GM103393). The contents of this publication are solely the
responsibility of the authors and do not necessarily represent the
official views of NIGMS or NIH.
NR 58
TC 7
Z9 7
U1 6
U2 56
PU AMER CHEMICAL SOC
PI WASHINGTON
PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA
SN 1932-7447
J9 J PHYS CHEM C
JI J. Phys. Chem. C
PD AUG 14
PY 2014
VL 118
IS 32
BP 18706
EP 18712
DI 10.1021/jp503941t
PG 7
WC Chemistry, Physical; Nanoscience & Nanotechnology; Materials Science,
Multidisciplinary
SC Chemistry; Science & Technology - Other Topics; Materials Science
GA AN2VQ
UT WOS:000340444500051
PM 25152800
ER
PT J
AU Galeazzi, M
Chiao, M
Collier, MR
Cravens, T
Koutroumpa, D
Kuntz, KD
Lallement, R
Lepri, ST
McCammon, D
Morgan, K
Porter, FS
Robertson, IP
Snowden, SL
Thomas, NE
Uprety, Y
Ursino, E
Walsh, BM
AF Galeazzi, M.
Chiao, M.
Collier, M. R.
Cravens, T.
Koutroumpa, D.
Kuntz, K. D.
Lallement, R.
Lepri, S. T.
McCammon, D.
Morgan, K.
Porter, F. S.
Robertson, I. P.
Snowden, S. L.
Thomas, N. E.
Uprety, Y.
Ursino, E.
Walsh, B. M.
TI The origin of the local 1/4-keV X-ray flux in both charge exchange and a
hot bubble
SO NATURE
LA English
DT Article
ID SOLAR-WIND; BACKGROUND FLUX; EMISSION; GAS; INFERENCES; MODEL
AB The solar neighbourhood is the closest and most easily studied sample of the Galactic interstellar medium, an understanding of which is essential for models of star formation and galaxy evolution. Observations of an unexpectedly intense diffuse flux of easily absorbed 1/4-kiloelectronvolt X-rays(1,2), coupled with the discovery that interstellar space within about a hundred parsecs of the Sun is almost completely devoid of cool absorbing gas(3), led to a picture of a 'local cavity' filled with X-ray-emitting hot gas, dubbed the local hot bubble(4-6). This model was recently challenged by suggestions that the emission could instead be readily produced within the Solar System by heavy solar-wind ions exchanging electrons with neutral H and He in interplanetary space(7-11), potentially removing the major piece of evidence for the local existence of million-degree gas within the Galactic disk(12-15). Here we report observations showing that the total solar-wind charge-exchange contribution is approximately 40 per cent of the 1/4-keV flux in the Galactic plane. The fact that the measured flux is not dominated by charge exchange supports the notion of a million-degree hot bubble extending about a hundred parsecs from the Sun.
C1 [Galeazzi, M.; Uprety, Y.; Ursino, E.] Univ Miami, Dept Phys, Coral Gables, FL 33124 USA.
[Chiao, M.; Collier, M. R.; Porter, F. S.; Snowden, S. L.; Thomas, N. E.; Walsh, B. M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Cravens, T.; Robertson, I. P.] Univ Kansas, Dept Phys & Astron, Lawrence, KS 66045 USA.
[Koutroumpa, D.] Univ Paris 06, Sorbonne Univ, Univ Versailles St Quentin, CNRS,INSU,LATMOS IPSL, F-78280 Guyancourt, France.
[Kuntz, K. D.] Johns Hopkins Univ, Henry A Rowland Dept Phys & Astron, Baltimore, MD 21218 USA.
[Lallement, R.] Univ Paris Diderot, GEPI Observ Paris, CNRS, UMR 8111, F-92190 Meudon, France.
[Lepri, S. T.] Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA.
[McCammon, D.; Morgan, K.] Univ Wisconsin, Dept Phys, Madison, WI 53706 USA.
RP Galeazzi, M (reprint author), Univ Miami, Dept Phys, Coral Gables, FL 33124 USA.
EM galeazzi@physics.miami.edu
RI Uprety, Youaraj/C-8104-2015; Porter, Frederick/D-3501-2012; Walsh,
Brian/C-4899-2016; Morgan, Kelsey/J-5053-2016; Collier,
Michael/I-4864-2013
OI Uprety, Youaraj/0000-0001-9101-2063; Porter,
Frederick/0000-0002-6374-1119; Walsh, Brian/0000-0001-7426-5413; Morgan,
Kelsey/0000-0002-6597-1030; Collier, Michael/0000-0001-9658-6605
FU NASA [NNX11AF04G, NNX09AF09G]; French space agency CNES; National
Program 'Physique Chimie du Milieu Interstellaire' of the Institut
National des Sciences de l'Univers (INSU)
FX We thank the personnel at NASA's Wallops Flight Facility and the White
Sands Military Range for their support of payload development,
integration and launch, and the technical personnel at the University of
Miami, NASA's Goddard Space Flight Center and the University of Michigan
for their support of the instrument's development. This work was
supported by NASA award numbers NNX11AF04G and NNX09AF09G. D.K. and R.L.
acknowledge financial support for their activity through the programme
'Soleil Heliosphere Magnetosphere' of the French space agency CNES, and
the National Program 'Physique Chimie du Milieu Interstellaire' of the
Institut National des Sciences de l'Univers (INSU). M.C. and N.E.T. are
employed through the Center for Research and Exploration in Space
Science and Technology (CRESST) and the University of Maryland,
Baltimore County, Baltimore, Maryland, USA.
NR 24
TC 21
Z9 21
U1 0
U2 10
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 AUG 14
PY 2014
VL 512
IS 7513
BP 171
EP +
DI 10.1038/nature13525
PG 6
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA AM9KO
UT WOS:000340200700026
PM 25079321
ER
PT J
AU Thompson, MS
Christoffersen, R
Zega, TJ
Keller, LP
AF Thompson, Michelle S.
Christoffersen, Roy
Zega, Thomas J.
Keller, Lindsay P.
TI Microchemical and structural evidence for space weathering in soils from
asteroid Itokawa
SO EARTH PLANETS AND SPACE
LA English
DT Article
DE Hayabusa; Itokawa; Space weathering; Irradiation; Micrometeorite impact;
Airless body; Transmission electron microscopy; Sample return analysis
ID BEAM-INDUCED AMORPHIZATION; LUNAR REGOLITH; DUST PARTICLES; VAPOR
DEPOSITS; IRRADIATION; MGO-AL2O3-SIO2; CHONDRITES; INSIGHTS; SURFACE;
SAMPLES
AB Here we report microchemical and microstructural features indicative of space weathering in a particle returned from the surface of asteroid Itokawa by the Hayabusa mission. Space weathering features include partially and completely amorphous rims, chemically and structurally heterogeneous multilayer rims, amorphous surface islands, vesiculated rim textures, and nanophase iron particles. Solar-wind irradiation is likely responsible for the amorphization as well as the associated vesiculation of grain rims. The multilayer rims contain a nanocrystalline outer layer that is underlain by an amorphous inner layer, and both have compositions that are distinct from the underlying, crystalline orthopyroxene grain. The multilayer rim features could be derived from either radiation-induced sputter deposition or vapor deposition from micrometeorite impact events. The amorphous islands on grain surfaces have a distinctive morphology and composition suggesting that they represent surface deposits of melt derived from micrometeorite impact events. These observations indicate that both irradiation damage and micrometeorite impacts play a role in surface modification and space weathering on asteroid Itokawa.
C1 [Thompson, Michelle S.; Zega, Thomas J.] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA.
[Christoffersen, Roy] NASA, Lyndon B Johnson Space Ctr, Mail Code KR, Houston, TX 77058 USA.
[Keller, Lindsay P.] NASA, JSC Mail Code KR, Houston, TX 77058 USA.
RP Thompson, MS (reprint author), Univ Arizona, Lunar & Planetary Lab, 1629 E Univ Blvd, Tucson, AZ 85721 USA.
EM mst@lpl.arizona.edu
FU NASA Laboratory Analysis of Returned Samples (LARS) program; Natural
Sciences and Engineering Research Council of Canada (NSERC); NASA
FX We thank JAXA for the allocation of Hayabusa samples for this study. We
gratefully acknowledge the use of facilities within the Leroy Eyring
Center for Solid State Science at Arizona State University. We
acknowledge the use of facilities and assistance from Huikai Cheng at
FEI. The TEM work at the Johnson Space Center was supported in part by a
grant to LPK from the NASA Laboratory Analysis of Returned Samples
(LARS) program. Funding for MS Thompson is provided by the Natural
Sciences and Engineering Research Council of Canada (NSERC). This
research was supported in part by NASA. Three anonymous reviewers are
acknowledged for their constructive comments.
NR 31
TC 11
Z9 11
U1 2
U2 8
PU SPRINGER HEIDELBERG
PI HEIDELBERG
PA TIERGARTENSTRASSE 17, D-69121 HEIDELBERG, GERMANY
SN 1880-5981
J9 EARTH PLANETS SPACE
JI Earth Planets Space
PD AUG 13
PY 2014
VL 66
AR 89
DI 10.1186/1880-5981-66-89
PG 10
WC Geosciences, Multidisciplinary
SC Geology
GA AQ9UW
UT WOS:000343203500001
ER
PT J
AU Klebanoff, LE
Breit, J
Roe, GS
Damberger, T
Erbel, T
Wingert, S
Coleman, B
Radley, CJ
Oros, JM
Schuttinger, P
Woolley, R
Ghotb, H
Prey, S
Velinsky, S
White, W
Saunders, R
Saunders, C
Drake, R
Rea, G
Fliess, D
Hooson, R
Elrick, WT
Hamilton, J
Skradski, T
Brown, G
Chao, B
Zelinsky, M
Sorkin, A
McGlaughlin, R
Moreland, G
Hanley, RC
Koonce, M
Johnson, TA
AF Klebanoff, L. E.
Breit, Js.
Roe, G. S.
Damberger, T.
Erbel, T.
Wingert, S.
Coleman, B.
Radley, C. J.
Oros, J. M.
Schuttinger, P.
Woolley, R.
Ghotb, H.
Prey, S.
Velinsky, S.
White, W.
Saunders, R.
Saunders, C.
Drake, R.
Rea, G.
Fliess, D.
Hooson, R.
Elrick, W. T.
Hamilton, J.
Skradski, T.
Brown, G.
Chao, B.
Zelinsky, M.
Sorkin, A.
McGlaughlin, R.
Moreland, G.
Hanley, R. C.
Koonce, M.
Johnson, T. A.
TI Fuel cell mobile lighting: A fuel cell market transformation project
SO INTERNATIONAL JOURNAL OF HYDROGEN ENERGY
LA English
DT Article
DE Fuel cell; Market transformation; Mobile lighting; Construction
equipment; Ground support equipment
AB We report the results of a project aimed to introduce proton exchange membrane (PEM) hydrogen fuel cell technology into aviation ground support equipment (GSE) and rental construction equipment. The purpose of the project was to design, build, field-test and then commercialize fuel cell equipment that is superior to its diesel counterpart. The commercializing of this hydrogen-based technology will help to start the process of displacing diesel fuel use in aviation GSE and in mobile construction equipment. We describe a hydrogen fuel cell mobile lighting tower (H2LT) that combines hydrogen stored as a high pressure gas, PEM fuel cell technology, and advanced lighting into a single unit with uses in aviation and construction. We assembled a project team of 15 institutional partners combining new technology expertise (hydrogen, fuel cells), equipment mass manufacturing capability (mobile light towers, lighting) and influential end-users to field test the H2LT in real-world use in diverse environments. Seed funding provided by Boeing enabled additional funding from the U.S. Department of Energy (DOE) and a preponderance of in-kind contributions from the industrial partners. Prototype units were constructed and field tested in the entertainment industry, at the San Francisco International Airport, at the NASA Kennedy Space Center, with the California Department of Transportation (Caltrans), and with the Connecticut Department of Transportation. The goals of these approximately year-long field tests were to assess operation of the H2LT technology in a wide variety of potentially corrosive environments (cold, wet, hot, humid, salty air) performing a wide variety of tasks, to reduce diesel emissions at these locations, and to help promote hydrogen PEM technology in new influential markets. The H2LT proved to be exceptionally durable in these diverse environments, demonstrating the compatibility of PEM fuel cells and high-pressure hydrogen storage with the construction equipment application. Results from the field tests are discussed, including system performance (efficiency, duration, durability) and the efficacy of refueling the system by different methods (H-2 stations, mobile refueling). The H2LT system is compared directly to a comparable diesel-fueled light tower with regard to size, performance and emissions savings. Overall, end users were pleased with the performance of the H2LT, noting the lack of emissions and exceptionally low noise level. Recommendations for improvement were also collected and will be discussed. Two types of lighting used on the H2LT (plasma, LED) were characterized by U.C. Davis in collaboration with Caltrans. LED lighting was found to be the most energy efficient and robust lighting technology for the highly mobile H2LT application. The technical "lessons-learned" are reviewed, along with the plans for commercialization of the H2LT technology by Multiquip Inc. Finally, the benefits to the industrial participants of the project organization are described. Copyright (C) 2014, Hydrogen Energy Publications, LLC. Published by Elsevier Ltd. All rights reserved.
C1 [Klebanoff, L. E.; Johnson, T. A.] Sandia Natl Labs, Livermore, CA 94551 USA.
[Breit, Js.; Roe, G. S.] Boeing Commercial Airplanes, Syst Concept Ctr, Everett, WA 98203 USA.
[Damberger, T.] Golden State Energy, Carson City, NV 89703 USA.
[Erbel, T.; Wingert, S.; Coleman, B.] Multiquip Inc, Carson, CA 90746 USA.
[Radley, C. J.; Oros, J. M.; Schuttinger, P.] Altergy Syst, Folsom, CA 95630 USA.
[Woolley, R.; Ghotb, H.; Prey, S.] Caltrans Div Res, Innovat & Syst Informat Technol Applicat Off, Irvine, CA 92612 USA.
[Velinsky, S.; White, W.] Univ Calif Davis, Dept Mech & Aerosp Engn, Davis, CA 95616 USA.
[Saunders, R.; Saunders, C.] Saunders Elect Inc, Arleta, CA 91331 USA.
[Drake, R.; Rea, G.] Stray Light Opt Technol Inc, Scottsburg, IN 47170 USA.
[Fliess, D.; Hooson, R.] San Francisco Int Airport, City & Cty San Francisco, San Francisco, CA 94128 USA.
[Elrick, W. T.; Hamilton, J.] Calif Fuel Cell Partnership, West Sacramento, CA 95691 USA.
[Skradski, T.] Lumenworks, Oakland, CA 94610 USA.
[Brown, G.] Luxirn Corp, Santa Clara, CA 95054 USA.
[Chao, B.; Zelinsky, M.] Ovon Hydrogen Syst, Rochester Hills, MI 48309 USA.
[Sorkin, A.; McGlaughlin, R.] NASA, TEERM Principal Ctr, Kennedy Space Ctr, FL 32899 USA.
[Moreland, G.] SRA Int, Latham, NY USA.
[Hanley, R. C.] Connecticut Dept Transportat, Newington, CT 06131 USA.
[Koonce, M.] IGX Grp Inc, San Francisco, CA 94102 USA.
RP Klebanoff, LE (reprint author), Sandia Natl Labs, POB 969,MS 9161,7011 East Ave, Livermore, CA 94551 USA.
EM lekleba@sandia.gov
FU Boeing Company [SC02/1651.14.00]; Fuel Cell Market Transformation
Program at the U.S. DOE Fuel Cell Technologies Office; DOE; Division of
Research and Innovation at Caltrans (under the direction of Larry
Orcutt); U.C. Davis AHMCT; NASA KSC; U.S. Department of Energy's
National Nuclear Security Administration [DE-AC04-94AL85000]
FX Partial funding from the Boeing Company is gratefully acknowledged via
the Boeing/Sandia CRADA SC02/1651.14.00. Funding from the Fuel Cell
Market Transformation Program (led by Pete Devlin) at the U.S. DOE Fuel
Cell Technologies Office was critical, making the broader and stronger
development project possible, and specifically allowing the construction
and field testing of five additional H2LT units. In addition
to funding, we appreciate the encouragement of Pete and his colleagues
Nancy Garland and John Christensen in the Market Transformation program.
Special thanks to Sunita Satyapal at DOE for supporting this work. The
authors thank Tien Nguyen of DOE for providing an analysis of GHG
emissions for the H2LT technology, with the hydrogen derived
from either steam reforming of natural gas, or wind-based electrolysis
of water.; The project would not have been successful without the
participation of Caltrans. We thank Randy Iwasaki, former director of
Caltrans, for providing wonderful encouragement and support of the work
in its early phases, and offering resources of the Division of Research
and Innovation at Caltrans (under the direction of Larry Orcutt) to be
applied in support of the project. Larry Orcutt directed Nancy Chinlund
of Caltrans to become involved. Nancy was very proactive in launching
the project from a Caltrans perspective, which led directly to Randy
Woolley's involvement in the project. The Caltrans partners aggressively
challenged the project to build a prototype in a few months' time to be
shown at the 2009 AASHTO meeting.; Caltrans provided considerable
in-kind support through the donation of its own technical expertise and
through its support of the U.C. Davis AHMCT for characterizing the
lighting options for the H2LT as well as supervising the
Caltrans District 3 field test. We acknowledge the contributions of
Gonzalo Gomez of Caltrans for discussions of lighting technology options
for the H2LT. Ben Creed, Lauren Miller, Sean Donohoe and Matt
Jones at U.C. Davis provided many hours of night work characterizing the
illumination provided by the candidate plasma, LED and MH lighting
options. In a related activity, Ty Larson of Boeing performed checks
that the glass covering the plasma lights was sufficiently absorbing UV
radiation, which was very helpful.; The staff at Saunders Electric,
including Ron Brewer, Frank Soggiu and Pat Hess were instrumental in the
3-year field tests of the Alpha and Beta H2LT units used for
the Los Angeles entertainment award shows and elsewhere in the
entertainment industry.; The field test of the unit at the NASA KSC was
an excellent example of cooperation between government agencies. We
thank Chuck Griffin for providing local supervision of the project from
the NASA KSC end, along with a lot of help from Melissa Clevenger of the
propellants group and Ray Davis from operations. The KSC staff were
extremely professional and helpful. We thank Pattie Lewis Burford (ITB
Inc.) and Jerry Curran (EASI) for providing corrosion inspection of the
Beta unit that was field tested at the NASA KSC for a year, and Randy
Morris for extensive coordination.; Sandia National Laboratories is a
multi-program laboratory managed and operated by Sandia Corporation, a
wholly owned subsidiary of Lockheed Martin Corporation, for the U.S.
Department of Energy's National Nuclear Security Administration under
contract DE-AC04-94AL85000.
NR 9
TC 3
Z9 3
U1 0
U2 23
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0360-3199
EI 1879-3487
J9 INT J HYDROGEN ENERG
JI Int. J. Hydrog. Energy
PD AUG 13
PY 2014
VL 39
IS 24
BP 12948
EP 12972
DI 10.1016/j.ijhydene.2014.05.180
PG 25
WC Chemistry, Physical; Electrochemistry; Energy & Fuels
SC Chemistry; Electrochemistry; Energy & Fuels
GA AN6FI
UT WOS:000340689900058
ER
PT J
AU Tucker, PG
DeBonis, JR
AF Tucker, P. G.
DeBonis, J. R.
TI Aerodynamics, computers and the environment
SO PHILOSOPHICAL TRANSACTIONS OF THE ROYAL SOCIETY A-MATHEMATICAL PHYSICAL
AND ENGINEERING SCIENCES
LA English
DT Editorial Material
DE large eddy simulation; aerodynamics; turbulence
C1 [Tucker, P. G.] Univ Cambridge, Dept Engn, Cambridge CB2 1PZ, England.
[DeBonis, J. R.] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA.
RP Tucker, PG (reprint author), Univ Cambridge, Dept Engn, Cambridge CB2 1PZ, England.
EM pgt23@cam.ac.uk
NR 16
TC 3
Z9 3
U1 1
U2 12
PU ROYAL SOC
PI LONDON
PA 6-9 CARLTON HOUSE TERRACE, LONDON SW1Y 5AG, ENGLAND
SN 1364-503X
EI 1471-2962
J9 PHILOS T R SOC A
JI Philos. Trans. R. Soc. A-Math. Phys. Eng. Sci.
PD AUG 13
PY 2014
VL 372
IS 2022
SI SI
AR 20130331
DI 10.1098/rsta.2013.0331
PG 5
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA AL0VJ
UT WOS:000338844700013
PM 25024420
ER
PT J
AU Vitale, S
Congedo, G
Dolesi, R
Ferroni, V
Hueller, M
Vetrugno, D
Weber, WJ
Audley, H
Danzmann, K
Diepholz, I
Hewitson, M
Korsakova, N
Ferraioli, L
Gibert, F
Karnesis, N
Nofrarias, M
Inchauspe, H
Plagnol, E
Jennrich, O
McNamara, PW
Armano, M
Thorpe, JI
Wass, P
AF Vitale, Stefano
Congedo, Giuseppe
Dolesi, Rita
Ferroni, Valerio
Hueller, Mauro
Vetrugno, Daniele
Weber, William Joseph
Audley, Heather
Danzmann, Karsten
Diepholz, Ingo
Hewitson, Martin
Korsakova, Natalia
Ferraioli, Luigi
Gibert, Ferran
Karnesis, Nikolaos
Nofrarias, Miquel
Inchauspe, Henri
Plagnol, Eric
Jennrich, Oliver
McNamara, Paul W.
Armano, Michele
Thorpe, James Ira
Wass, Peter
TI Data series subtraction with unknown and unmodeled background noise
SO PHYSICAL REVIEW D
LA English
DT Article
AB LISA Pathfinder (LPF), the precursor mission to a gravitational wave observatory of the European Space Agency, will measure the degree to which two test masses can be put into free fall, aiming to demonstrate a suppression of disturbance forces corresponding to a residual relative acceleration with a power spectral density (PSD) below (30 fm/s(2)/root Hz)(2) around 1 mHz. In LPF data analysis, the disturbance forces are obtained as the difference between the acceleration data and a linear combination of other measured data series. In many circumstances, the coefficients for this linear combination are obtained by fitting these data series to the acceleration, and the disturbance forces appear then as the data series of the residuals of the fit. Thus the background noise or, more precisely, its PSD, whose knowledge is needed to build up the likelihood function in ordinary maximum likelihood fitting, is here unknown, and its estimate constitutes instead one of the goals of the fit. In this paper we present a fitting method that does not require the knowledge of the PSD of the background noise. The method is based on the analytical marginalization of the posterior parameter probability density with respect to the background noise PSD, and returns an estimate both for the fitting parameters and for the PSD. We show that both these estimates are unbiased, and that, when using averaged Welch's periodograms for the residuals, the estimate of the PSD is consistent, as its error tends to zero with the inverse square root of the number of averaged periodograms. Additionally, we find that the method is equivalent to some implementations of iteratively reweighted least-squares fitting. We have tested the method both on simulated data of known PSD and on data from several experiments performed with the LISA Pathfinder end-to-end mission simulator.
C1 [Vitale, Stefano; Congedo, Giuseppe; Dolesi, Rita; Ferroni, Valerio; Hueller, Mauro; Vetrugno, Daniele; Weber, William Joseph] Univ Trento, Dept Phys, I-38123 Povo, Trento, Italy.
[Vitale, Stefano; Congedo, Giuseppe; Dolesi, Rita; Ferroni, Valerio; Hueller, Mauro; Vetrugno, Daniele; Weber, William Joseph] Ist Nazl Fis Nucl, Trento Inst Fundamental Phys & Applicat, I-38123 Povo, Trento, Italy.
[Audley, Heather; Danzmann, Karsten; Diepholz, Ingo; Hewitson, Martin; Korsakova, Natalia] Max Planck Inst Gravitat Phys, Albert Einstein Inst, D-30167 Hannover, Germany.
[Audley, Heather; Danzmann, Karsten; Diepholz, Ingo; Hewitson, Martin; Korsakova, Natalia] Leibniz Univ Hannover, D-30167 Hannover, Germany.
[Ferraioli, Luigi] ETH, Inst Geophys, CH-8092 Zurich, Switzerland.
[Gibert, Ferran; Karnesis, Nikolaos; Nofrarias, Miquel] CSIC IEEC, Fac Ciencies, Inst Ciencies Espai, Bellaterra 08193, Spain.
[Inchauspe, Henri; Plagnol, Eric] Univ Paris Diderot, APC, CNRS IN2P3, CEA Ifru,Observ Paris,Sorbonne Paris Cite, F-75205 Paris 13, France.
[Jennrich, Oliver; McNamara, Paul W.] European Space Agcy, European Space Technol Ctr, NL-2200 AG Noordwijk, Netherlands.
[Armano, Michele] European Space Agcy, European Space Astron Ctr, Madrid 28692, Spain.
[Thorpe, James Ira] NASA, Goddard Space Flight Ctr, Gravitat Astrophys Lab, Greenbelt, MD 20771 USA.
[Wass, Peter] Univ London Imperial Coll Sci Technol & Med, Blackett Lab, High Energy Phys Grp, London SW7 2AZ, England.
RP Vitale, S (reprint author), Univ Trento, Dept Phys, I-38123 Povo, Trento, Italy.
EM stefano.vitale@unitn.it
RI Weber, William/H-4351-2012; Vitale, Stefano/C-2312-2012; Nofrarias,
Miquel/N-6249-2015; Wass, Peter/C-5767-2017
OI Weber, William/0000-0003-1536-2410; Vitale, Stefano/0000-0002-2427-8918;
Nofrarias, Miquel/0000-0003-1518-2196; Wass, Peter/0000-0002-2945-399X
FU Agenzia Spaziale Italiana; Istituto Nazionale di Fisica Nucleare;
Deutsches Zentrum fur Luft- und Raumfahrt e.V.; Swiss Space Office;
State Secretariat for Education, Research and Innovation; United Kingdom
Space Agency; Plan Nacional del Espacio of the Spanish Ministry of
Science and Innovation; Centre Nationale d'Etudes Spatiales
FX This work has been supported in part under contracts from Agenzia
Spaziale Italiana, Istituto Nazionale di Fisica Nucleare, Deutsches
Zentrum fur Luft- und Raumfahrt e.V., Swiss Space Office, State
Secretariat for Education, Research and Innovation, United Kingdom Space
Agency, Plan Nacional del Espacio of the Spanish Ministry of Science and
Innovation, and Centre Nationale d'Etudes Spatiales.
NR 18
TC 8
Z9 8
U1 1
U2 13
PU AMER PHYSICAL SOC
PI COLLEGE PK
PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA
SN 1550-7998
EI 1550-2368
J9 PHYS REV D
JI Phys. Rev. D
PD AUG 11
PY 2014
VL 90
IS 4
AR 042003
DI 10.1103/PhysRevD.90.042003
PG 15
WC Astronomy & Astrophysics; Physics, Particles & Fields
SC Astronomy & Astrophysics; Physics
GA AO3SG
UT WOS:000341255200001
ER
PT J
AU Pierens, A
Raymond, SN
AF Pierens, A.
Raymond, S. N.
TI Disruption of co-orbital (1:1) planetary resonances during gas-driven
orbital migration
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE accretion, accretion discs; hydrodynamics; methods: numerical; planets
and satellites: formation; planet-disc interactions
ID MEAN-MOTION RESONANCES; TRANSITING EXTRASOLAR PLANETS; OUTWARD
MIGRATION; PROTOSTELLAR DISC; TROJAN PLANETS; SUPER-EARTHS; SYSTEMS;
PROTOPLANETS; NEBULA; MASS
AB Planets close to their stars are thought to form farther out and migrate inwards due to angular momentum exchange with gaseous protoplanetary discs. This process can produce systems of planets in co-orbital (Trojan or 1:1) resonance, in which two planets share the same orbit, usually separated by 60 deg. Co-orbital systems are detectable among the planetary systems found by the Kepler mission either directly or by transit timing variations. However, no co-orbital systems have been found within the thousands of Kepler planets and candidates. Here, we study the orbital evolution of co-orbital planets embedded in a protoplanetary disc using a grid-based hydrodynamics code. We show that pairs of similar-mass planets in co-orbital resonance are disrupted during large-scale orbital migration. Destabilization occurs when one or both planets are near the critical mass needed to open a gap in the gaseous disc. A confined gap is opened that spans the 60 deg azimuthal separation between planets. This alters the torques imparted by the disc on each planet - pushing the leading planet outwards and the trailing planet inwards - and disrupts the resonance. The mechanism applies to systems in which the two planets' masses differ by a factor of 2 or less. In a simple flared disc model, the critical mass for gap opening varies from a few Earth masses at the inner edge of the disc to 1 Saturn mass at 5 au. A pair of co-orbital planets with masses in this range that migrates will enter a region where the planets are at the gap-opening limit. At that point, the resonance is disrupted. We therefore predict an absence of planets on co-orbital configurations with masses in the super-Earth to Saturn mass range with similar masses.
C1 [Pierens, A.; Raymond, S. N.] Univ Bordeaux, Observ Aquitain Sci Univers, F-33271 Floirac, France.
[Pierens, A.; Raymond, S. N.] CNRS, Lab Astrophys Bordeaux, F-33271 Floirac, France.
[Raymond, S. N.] NASA, Astrobiol Inst, Virtual Planetary Lab, Washington, DC USA.
RP Pierens, A (reprint author), Univ Bordeaux, Observ Aquitain Sci Univers, F-BP89, F-33271 Floirac, France.
EM arnaud.pierens@obs.u-bordeaux1.fr
FU Agence Nationale pour la Recherche [ANR-13-BS05-0003]; NASA [NNA13AA93A]
FX Computer time for this study was provided by the computing facilities
MCIA (Mesocentre de Calcul Intensif Aquitain) of the Universite de
Bordeaux and by HPC resources of Cines under the allocation c2013046957
made by GENCI (Grand Equipement National de Calcul Intensif). We thank
the Agence Nationale pour la Recherche under grant ANR-13-BS05-0003
(MOJO). SNR's contribution was performed as part of the NASA
Astrobiology Institute's Virtual Planetary Laboratory Lead Team,
supported by the NASA under Cooperative Agreement no. NNA13AA93A.
NR 51
TC 3
Z9 3
U1 0
U2 1
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 AUG 11
PY 2014
VL 442
IS 3
BP 2296
EP 2303
DI 10.1093/mnras/stu1008
PG 8
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AM5TU
UT WOS:000339924300030
ER
PT J
AU Pretorius, ML
Mukai, K
AF Pretorius, Magaretha L.
Mukai, Koji
TI Constraints on the space density of intermediate polars from the
Swift-BAT survey
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE methods: observational; methods: statistical; novae; cataclysmic
variables; X-rays: binaries
ID MAGNETIC CATACLYSMIC VARIABLES; ALPHA-SELECTED SAMPLE; PALOMAR-GREEN
SAMPLE; X-RAY BINARIES; TV-COLUMBAE; SYSTEM PARAMETERS; ACCRETION RATE;
HST PARALLAX; PQ-GEMINORUM; DONOR STARS
AB We construct a complete, hard X-ray flux-limited sample of intermediate polars (IPs) from the Swift-BAT 70-month survey, by imposing selection cuts in flux and Galactic latitude (F-X > 2.5 x 10(- 11) erg cm(- 2) s(- 1) at 14-195 keV, and |b| > 5A degrees). We then use it to estimate the space density (rho) of IPs. Assuming that this sample of 15 long-period systems is representative of the intrinsic IP population, the space density of long-period IPs is 1-(+1)(0.5) x 10(-7) pc(-3). The Swift-BAT data also allow us to place upper limits on the size of a hypothetical population of faint IPs that is not included in the flux-limited sample. While most IPs detected by Swift-BAT have 14-195 keV luminosities of similar to 10(33) erg s(-1), there is evidence of a fainter population at L-X similar to 10(31) erg s(- 1). We find that a population of IPs with this luminosity may have a space density as large as 5 x 10(-6) pc(-3). Furthermore, these low-luminosity IPs, despite appearing rare in observed samples, are probably at least as intrinsically common as the brighter systems that are better represented in the known IP sample.
C1 [Pretorius, Magaretha L.] Univ Oxford, Dept Phys, Oxford OX1 3RH, England.
[Mukai, Koji] CRESST, Greenbelt, MD 20771 USA.
[Mukai, Koji] NASA, Xray Astrophys Lab, GSFC, Greenbelt, MD 20771 USA.
[Mukai, Koji] Univ Maryland Baltimore Cty, Dept Phys, Baltimore, MD 21250 USA.
RP Pretorius, ML (reprint author), Univ Oxford, Dept Phys, Denys Wilkinson Bldg,Keble Rd, Oxford OX1 3RH, England.
EM retha.pretorius@astro.ox.ac.uk
FU Marie Curie International Incoming Fellowship [PIIF-GA-2012-328716]
FX MLP is funded by a Marie Curie International Incoming Fellowship within
the 7th European Community Framework Programme (grant no.
PIIF-GA-2012-328716).
NR 64
TC 13
Z9 13
U1 0
U2 0
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 AUG 11
PY 2014
VL 442
IS 3
BP 2580
EP 2585
DI 10.1093/mnras/stu990
PG 6
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AM5TU
UT WOS:000339924300052
ER
PT J
AU Walker, ES
Mazzali, PA
Pian, E
Hurley, K
Arcavi, I
Cenko, SB
Gal-Yam, A
Horesh, A
Kasliwal, M
Poznanski, D
Silverman, JM
Sullivan, M
Bloom, JS
Filippenko, AV
Kulkarni, SR
Nugent, PE
Ofek, E
Barthelmy, S
Boynton, W
Goldsten, J
Golenetskii, S
Ohno, M
Tashiro, MS
Yamaoka, K
Zhang, XL
AF Walker, E. S.
Mazzali, P. A.
Pian, E.
Hurley, K.
Arcavi, I.
Cenko, S. B.
Gal-Yam, A.
Horesh, A.
Kasliwal, M.
Poznanski, D.
Silverman, J. M.
Sullivan, M.
Bloom, J. S.
Filippenko, A. V.
Kulkarni, S. R.
Nugent, P. E.
Ofek, E.
Barthelmy, S.
Boynton, W.
Goldsten, J.
Golenetskii, S.
Ohno, M.
Tashiro, M. S.
Yamaoka, K.
Zhang, X. L.
TI Optical follow-up observations of PTF10qts, a luminous broad-lined Type
Ic supernova found by the Palomar Transient Factory
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE supernovae: general; supernovae: individual: PTF10qts
ID GAMMA-RAY BURST; CORE-COLLAPSE SUPERNOVAE; LIGHT-CURVE; SN 1998BW;
LOW-METALLICITY; DWARF GALAXIES; GRB 100316D; HYPERNOVA; GRB-031203;
PHOTOMETRY
AB We present optical photometry and spectroscopy of the broad-lined Type Ic supernova (SN Ic-BL) PTF10qts, which was discovered as part of the Palomar Transient Factory. The SN was located in a dwarf galaxy of magnitude r = 21.1 at a redshift z = 0.0907. We find that the R-band light curve is a poor proxy for bolometric data and use photometric and spectroscopic data to construct and constrain the bolometric light curve. The derived bolometric magnitude at maximum light is M-bol = -18.51 +/- 0.2 mag, comparable to that of SN 1998bw (M-bol = -18.7 mag) which was associated with a gamma-ray burst (GRB). PTF10qts is one of the most luminous SNe Ic-BL observed without an accompanying GRB. We estimate the physical parameters of the explosion using data from our programme of follow-up observations, finding that it produced a larger mass of radioactive nickel compared to other SNe Ic-BL with similar inferred ejecta masses and kinetic energies. The progenitor of the event was likely an similar to 20 M-aS (TM) star.
C1 [Walker, E. S.; Pian, E.] Scuola Normale Super Pisa, I-56126 Pisa, Italy.
[Walker, E. S.] Yale Univ, Dept Phys, New Haven, CT 06520 USA.
[Mazzali, P. A.] Liverpool John Moores Univ, Astrophys Res Inst, Liverpool L3 5RF, Merseyside, England.
[Mazzali, P. A.] INAF Padova Astron Observ, I-35122 Padua, Italy.
[Mazzali, P. A.] Max Planck Inst Astrophys, D-85741 Garching, Germany.
[Pian, E.] INAF IASF, I-40129 Bologna, Italy.
[Pian, E.] Ist Nazl Fis Nucl, Sez Pisa, I-56127 Pisa, Italy.
[Hurley, K.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
[Arcavi, I.; Gal-Yam, A.; Ofek, E.] Weizmann Inst Sci, Dept Particle Phys & Astrophys, IL-76100 Rehovot, Israel.
[Cenko, S. B.; Barthelmy, S.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Cenko, S. B.; Bloom, J. S.; Filippenko, A. V.; Nugent, P. E.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA.
[Horesh, A.; Kulkarni, S. R.] CALTECH, Cahill Ctr Astrophys, Pasadena, CA 91125 USA.
[Kasliwal, M.] Carnegie Princeton Fellow, Pasadena, CA 91101 USA.
[Poznanski, D.] Tel Aviv Univ, Sch Phys & Astron, IL-69978 Tel Aviv, Israel.
[Silverman, J. M.] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA.
[Sullivan, M.] Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England.
[Nugent, P. E.] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Berkeley, CA 94720 USA.
[Boynton, W.] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA.
[Goldsten, J.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA.
[Golenetskii, S.] Russian Acad Sci, Ioffe Physicotech Inst, St Petersburg 194021, Russia.
[Ohno, M.] Hiroshima Univ, Dept Phys Sci, Hiroshima 7398526, Japan.
[Tashiro, M. S.] Saitama Univ, Dept Phys, Sakura Ku, Saitama 3388570, Japan.
[Yamaoka, K.] Aoyama Gakuin Univ, Dept Phys & Math, Sagamihara, Kanagawa 2298558, Japan.
[Zhang, X. L.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany.
RP Walker, ES (reprint author), Scuola Normale Super Pisa, Piazza Cavalieri 7, I-56126 Pisa, Italy.
EM emma.walker@yale.edu
RI Golenetskii, Sergey/B-3818-2015; Horesh, Assaf/O-9873-2016;
OI Horesh, Assaf/0000-0002-5936-1156; Sullivan, Mark/0000-0001-9053-4820;
Pian, Elena/0000-0001-8646-4858
FU ASI [I/016/07/0 (COFIS), I/088/06/0]; PRIN INAF; Minerva grant; ISF;
BSF; GIF; EU [307260]; Gary and Cynthia Bengier; Christopher R. Redlich
Fund; Richard and Rhoda Goldman Fund; TABASGO Foundation; NSF
[AST-1211916, AST-1302771]; Israeli Ministry of Science; I-CORE
programme of the Planning and Budgeting Committee; Israel Science
Foundation [1829/12]; W.M. Keck Foundation; NASA [NNX10AI23G (Swift),
NNX09AV61G (Suzaku), NNX09AU03G (Fermi), NNX09AR28G (INTEGRAL)]
FX We acknowledge financial contributions from contract ASI I/016/07/0
(COFIS), ASI I/088/06/0, and PRIN INAF 2009 and 2011. PTF is a
collaboration of Caltech, LCOGT, the Weizmann Institute, LBNL, Oxford,
Columbia, IPAC, and UC Berkeley. Collaborative work between AG and PAM
is supported by a Minerva grant. The Weizmann PTF membership is
supported by the ISF via grants to AG. Joint work of AG and SRK is
supported by a BSF grant. AG also acknowledges support by grants from
the GIF, EU/FP7 via ERC grant 307260, 'The Quantum Universe', I-CORE
programme by the Israeli Committee for planning and budgeting, the
Kimmel award, and the Lord Sieff of Brimpton Fund. AVF's group at UC
Berkeley has received generous financial assistance from Gary and
Cynthia Bengier, the Christopher R. Redlich Fund, the Richard and Rhoda
Goldman Fund, the TABASGO Foundation, and NSF grant AST-1211916. JMS is
supported by an NSF Astronomy and Astrophysics Postdoctoral Fellowship
under award AST-1302771. EOO is incumbent of the Arye Dissentshik career
development chair and is grateful to support by a grant from the Israeli
Ministry of Science and the I-CORE programme of the Planning and
Budgeting Committee and the Israel Science Foundation (grant No
1829/12).; We thank the very helpful staffs of the various observatories
(Palomar, Lick, KNPO, TNG, Keck) at which data were obtained. The W. M.
Keck Observatory is operated as a scientific partnership among the
California Institute of Technology, the University of California, and
NASA; it was made possible by the generous financial support of the W.M.
Keck Foundation. M.T. Kandrashoff and J. Rex assisted with the Lick
observations. We are grateful to the following contributors to the IPN
for support and sharing their data: I. G. Mitrofanov, D. Golovin, M. L.
Litvak, A. B. Sanin, C. Fellows, K. Harshman, and R. Starr (for the
Odyssey team), R. Aptekar, E. Mazets, V. Pal'shin, D. Frederiks, and D.
Svinkin (for the Konus-Wind team), A. von Kienlin and A. Rau (for the
INTEGRAL team), T. Takahashi, M. Ohno, Y. Hanabata, Y. Fukazawa, M.
Tashiro, Y. Terada, T. Murakami, and K. Makishima (for the Suzaku team),
T. Cline, J. Cummings, N. Gehrels, H. Krimm, and D. Palmer (for the
Swift team), and V. Connaughton, M. S. Briggs, and C. Meegan (for the
Fermi GBM team). KH acknowledges NASA support for the IPN under the
following grants: NNX10AI23G (Swift), NNX09AV61G (Suzaku), NNX09AU03G
(Fermi), and NNX09AR28G (INTEGRAL).
NR 83
TC 7
Z9 7
U1 1
U2 7
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 AUG 11
PY 2014
VL 442
IS 3
BP 2768
EP 2779
DI 10.1093/mnras/stu1017
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AM5TU
UT WOS:000339924300067
ER
PT J
AU Cudjoe, E
Nguyen, BN
Meador, MAB
Sandberg, A
Rowan, SJ
AF Cudjoe, Elvis
Nguyen, Baochau N.
Meador, Mary Ann B.
Sandberg, Anna
Rowan, Stuart J.
TI Polyimide cellulose nanocrystal composite aerogels
SO ABSTRACTS OF PAPERS OF THE AMERICAN CHEMICAL SOCIETY
LA English
DT Meeting Abstract
CT 248th National Meeting of the American-Chemical-Society (ACS)
CY AUG 10-14, 2014
CL San Francisco, CA
SP Amer Chem Soc
C1 [Cudjoe, Elvis; Rowan, Stuart J.] Case Western Reserve Univ, Cleveland, OH 44106 USA.
[Meador, Mary Ann B.; Sandberg, Anna] NASA Glenn Res Ctr, Cleveland, OH 44135 USA.
[Nguyen, Baochau N.] NASA Glenn Res Ctr, Ohio Aerosp Inst, Cleveland, OH 44135 USA.
EM exc229@case.edu
NR 0
TC 0
Z9 0
U1 3
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 AUG 10
PY 2014
VL 248
MA 295-PMSE
PG 1
WC Chemistry, Multidisciplinary
SC Chemistry
GA CA8KC
UT WOS:000349167404660
ER
PT J
AU Haskins, J
Bennett, WR
Hernandez-Lugo, DM
Wu, J
Borodin, O
Monk, JD
Bauschlicher, CW
Lawson, J
AF Haskins, Justin
Bennett, William R.
Hernandez-Lugo, Dione M.
Wu, James
Borodin, Oleg
Monk, Joshua D.
Bauschlicher, Charles W.
Lawson, John
TI Investigation of structure and transport in Li-doped ionic liquid
electrolytes: [pyr14][TFSI], [pyr13][FSI], and [EMIM][BF4]
SO ABSTRACTS OF PAPERS OF THE AMERICAN CHEMICAL SOCIETY
LA English
DT Meeting Abstract
CT 248th National Meeting of the American-Chemical-Society (ACS)
CY AUG 10-14, 2014
CL San Francisco, CA
SP Amer Chem Soc
C1 [Haskins, Justin; Monk, Joshua D.; Bauschlicher, Charles W.; Lawson, John] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Bennett, William R.; Hernandez-Lugo, Dione M.; Wu, James] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA.
[Borodin, Oleg] US Army Res Lab, Adelphi, MD 20783 USA.
EM justin.b.haskins@nasa.gov
RI Borodin, Oleg/B-6855-2012
OI Borodin, Oleg/0000-0002-9428-5291
NR 0
TC 0
Z9 0
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 AUG 10
PY 2014
VL 248
MA 629-PHYS
PG 1
WC Chemistry, Multidisciplinary
SC Chemistry
GA CA8KC
UT WOS:000349167404333
ER
PT J
AU Huang, XC
Schwenke, DW
Lee, TJ
Tashkun, SA
Gamache, RR
Freedman, RS
AF Huang, Xinchuan
Schwenke, David W.
Lee, Timothy J.
Tashkun, Sergey A.
Gamache, Robert R.
Freedman, Richard S.
TI Accurate infrared line lists computed for CO2 and SO2 isotopologues
SO ABSTRACTS OF PAPERS OF THE AMERICAN CHEMICAL SOCIETY
LA English
DT Meeting Abstract
CT 248th National Meeting of the American-Chemical-Society (ACS)
CY AUG 10-14, 2014
CL San Francisco, CA
SP Amer Chem Soc
C1 [Huang, Xinchuan; Freedman, Richard S.] SETI Inst, Mountain View, CA 94043 USA.
[Schwenke, David W.] NASA, Ames Res Ctr, NAS Facil, Moffett Field, CA 94035 USA.
[Lee, Timothy J.] NASA, Ames Res Ctr, Space Sci & Astrobiol Div, Moffett Field, CA 94035 USA.
[Tashkun, Sergey A.] VE Zuev Inst Atmospher Opt, Tomsk 634021, Russia.
[Gamache, Robert R.] Univ Massachusetts, Dept Environm Earth & Atmospher Sci, Lowell, MA 01854 USA.
EM xinchuan@gmail.com
RI HUANG, XINCHUAN/A-3266-2013; Tashkun, Sergey/E-8682-2014
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 AUG 10
PY 2014
VL 248
MA 256-PHYS
PG 1
WC Chemistry, Multidisciplinary
SC Chemistry
GA CA8KC
UT WOS:000349167403854
ER
PT J
AU Huang, XC
Lee, TJ
AF Huang, Xinchuan
Lee, Timothy J.
TI History of a theoretical spectroscopy package SPECTRO and its recent
applications in astrophysical studies
SO ABSTRACTS OF PAPERS OF THE AMERICAN CHEMICAL SOCIETY
LA English
DT Meeting Abstract
CT 248th National Meeting of the American-Chemical-Society (ACS)
CY AUG 10-14, 2014
CL San Francisco, CA
SP Amer Chem Soc
C1 [Huang, Xinchuan] SETI Inst, Mountain View, CA 94043 USA.
[Huang, Xinchuan] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Lee, Timothy J.] NASA, Ames Res Ctr, Space Sci & Astrobiol Div, Moffett Field, CA 94035 USA.
EM xinchuan@gmail.com
RI HUANG, XINCHUAN/A-3266-2013
NR 0
TC 0
Z9 0
U1 0
U2 2
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 AUG 10
PY 2014
VL 248
MA 472-COMP
PG 1
WC Chemistry, Multidisciplinary
SC Chemistry
GA CA8JN
UT WOS:000349165104675
ER
PT J
AU Hudson, R
AF Hudson, Reggie
TI Rise, fall, and fine print of Erlenmeyer's rule
SO ABSTRACTS OF PAPERS OF THE AMERICAN CHEMICAL SOCIETY
LA English
DT Meeting Abstract
CT 248th National Meeting of the American-Chemical-Society (ACS)
CY AUG 10-14, 2014
CL San Francisco, CA
SP Amer Chem Soc
C1 [Hudson, Reggie] NASA Goddard Space Flight Ctr, Astrochem Lab, Greenbelt, MD USA.
EM reggie.hudson@nasa.gov
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 AUG 10
PY 2014
VL 248
MA 5-HIST
PG 1
WC Chemistry, Multidisciplinary
SC Chemistry
GA CA8KC
UT WOS:000349167400392
ER
PT J
AU Hudson, RL
Gerakines, PA
AF Hudson, Reggie L.
Gerakines, Perry A.
TI Radiolytic destruction of amino acids from Mars to the interstellar
medium
SO ABSTRACTS OF PAPERS OF THE AMERICAN CHEMICAL SOCIETY
LA English
DT Meeting Abstract
CT 248th National Meeting of the American-Chemical-Society (ACS)
CY AUG 10-14, 2014
CL San Francisco, CA
SP Amer Chem Soc
C1 [Hudson, Reggie L.; Gerakines, Perry A.] NASA, Goddard Space Flight Ctr, Astrochem Lab Code 691, Greenbelt, MD 20771 USA.
EM reggie.hudson@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 AUG 10
PY 2014
VL 248
MA 219-PHYS
PG 1
WC Chemistry, Multidisciplinary
SC Chemistry
GA CA8KC
UT WOS:000349167403821
ER
PT J
AU Hui, AO
Grieman, FJ
Okumura, M
Sander, SP
AF Hui, Aileen O.
Grieman, Frederick J.
Okumura, Mitchio
Sander, Stanley P.
TI Laboratory experiments of HO2 reactions with peroxy radicals using
infrared kinetic spectroscopy (IRKS)
SO ABSTRACTS OF PAPERS OF THE AMERICAN CHEMICAL SOCIETY
LA English
DT Meeting Abstract
CT 248th National Meeting of the American-Chemical-Society (ACS)
CY AUG 10-14, 2014
CL San Francisco, CA
SP Amer Chem Soc
C1 [Hui, Aileen O.; Okumura, Mitchio] CALTECH, Dept Chem & Chem Engn, Pasadena, CA 91125 USA.
[Grieman, Frederick J.] Pomona Coll, Dept Chem, Claremont, CA 91711 USA.
[Hui, Aileen O.; Sander, Stanley P.] NASA, Jet Prop Lab, Pasadena, CA 91109 USA.
EM aileenh@caltech.edu
NR 4
TC 0
Z9 0
U1 2
U2 5
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 AUG 10
PY 2014
VL 248
MA 95-PHYS
PG 1
WC Chemistry, Multidisciplinary
SC Chemistry
GA CA8KC
UT WOS:000349167403700
ER
PT J
AU Liu, YD
Zhang, JS
Wang, LM
Troy, T
Ahmed, M
AF Liu, Yingdi
Zhang, Jingsong
Wang, Liming
Troy, Tyler
Ahmed, Musahid
TI Direct characterization of Criegee intermediate in ozonolysis reaction
of alkene
SO ABSTRACTS OF PAPERS OF THE AMERICAN CHEMICAL SOCIETY
LA English
DT Meeting Abstract
CT 248th National Meeting of the American-Chemical-Society (ACS)
CY AUG 10-14, 2014
CL San Francisco, CA
SP Amer Chem Soc
C1 [Liu, Yingdi] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Zhang, Jingsong] Univ Calif Riverside, Riverside, CA 92521 USA.
[Wang, Liming] S China Univ Technol, Sch Chem & Chem Engn, Guangzhou 510640, Guangdong, Peoples R China.
[Troy, Tyler; Ahmed, Musahid] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Div Chem Sci, Berkeley, CA 94720 USA.
EM yingdi@caltech.edu; jingsong.zhang@ucr.edu
NR 0
TC 0
Z9 0
U1 1
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 AUG 10
PY 2014
VL 248
MA 41-PHYS
PG 1
WC Chemistry, Multidisciplinary
SC Chemistry
GA CA8KC
UT WOS:000349167403647
ER
PT J
AU Liu, YD
Sander, SP
AF Liu, Yingdi
Sander, Stanley P.
TI Pressure and temperature dependences of rate coefficients for the
reaction OH + NO2 + M -> products
SO ABSTRACTS OF PAPERS OF THE AMERICAN CHEMICAL SOCIETY
LA English
DT Meeting Abstract
CT 248th National Meeting of the American-Chemical-Society (ACS)
CY AUG 10-14, 2014
CL San Francisco, CA
SP Amer Chem Soc
C1 [Liu, Yingdi; Sander, Stanley P.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
EM YINGDI@CALTECH.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 AUG 10
PY 2014
VL 248
MA 420-ENVR
PG 1
WC Chemistry, Multidisciplinary
SC Chemistry
GA CA8JN
UT WOS:000349165105839
ER
PT J
AU Mathies, R
Willis, P
Lillis, R
Amundson, R
Beegle, K
Butterworth, A
Curtis, D
Ehrenfreund, P
Grunthaner, FA
Hazen, R
Kaiser, RI
Kim, J
Ludham, M
Mora, M
Scherer, J
Stockton, A
Turin, P
Welten, K
Williford, K
AF Mathies, Richard
Willis, Peter
Lillis, Robert
Amundson, Ronald
Beegle, Kuther
Butterworth, Anna
Curtis, David
Ehrenfreund, Pascale
Grunthaner, Frank A.
Hazen, Robert
Kaiser, Ralf I.
Kim, Jungkyu
Ludham, Michael
Mora, Maria
Scherer, James
Stockton, Amanda
Turin, Paul
Welten, Kees
Williford, Kenneth
TI Mars organic analyzer: Methods and instrumentation for detecting trace
organic molecules in our solar system
SO ABSTRACTS OF PAPERS OF THE AMERICAN CHEMICAL SOCIETY
LA English
DT Meeting Abstract
CT 248th National Meeting of the American-Chemical-Society (ACS)
CY AUG 10-14, 2014
CL San Francisco, CA
SP Amer Chem Soc
C1 [Mathies, Richard; Grunthaner, Frank A.; Scherer, James] Univ Calif Berkeley, Dept Chem, Berkeley, CA 94720 USA.
[Willis, Peter; Beegle, Kuther; Mora, Maria; Stockton, Amanda; Williford, Kenneth] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Lillis, Robert; Butterworth, Anna; Curtis, David; Ludham, Michael; Turin, Paul; Welten, Kees] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
[Amundson, Ronald] Univ Calif Berkeley, Dept Environm Sci, Berkeley, CA 94720 USA.
[Ehrenfreund, Pascale] George Washington Univ, Inst Space Policy, Washington, DC 20052 USA.
[Hazen, Robert] Geophys Lab, Washington, DC 20052 USA.
[Kaiser, Ralf I.] Univ Hawaii Manoa, Dept Chem, Honolulu, HI 96822 USA.
[Kim, Jungkyu] Texas Tech Univ, Dept Mech Engn, Lubbock, TX 79409 USA.
EM ramathies@berkeley.edu
RI Willis, Peter/I-6621-2012; Lillis, Robert/A-3281-2008
OI Lillis, Robert/0000-0003-0578-517X
NR 0
TC 0
Z9 0
U1 2
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 AUG 10
PY 2014
VL 248
MA 104-PHYS
PG 1
WC Chemistry, Multidisciplinary
SC Chemistry
GA CA8KC
UT WOS:000349167403709
ER
PT J
AU Meador, MAB
Guo, HQ
Nguyen, B
Williams, JC
Vivod, SL
AF Meador, Mary Ann B.
Guo, Haiquan
Baochau Nguyen
Williams, Jarrod C.
Vivod, Stephanie L.
TI Recent advances in design of polymer aerogels for aerospace applications
SO ABSTRACTS OF PAPERS OF THE AMERICAN CHEMICAL SOCIETY
LA English
DT Meeting Abstract
CT 248th National Meeting of the American-Chemical-Society (ACS)
CY AUG 10-14, 2014
CL San Francisco, CA
SP Amer Chem Soc
C1 [Meador, Mary Ann B.; Guo, Haiquan; Baochau Nguyen; Williams, Jarrod C.; Vivod, Stephanie L.] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA.
EM maryann.meador@nasa.gov
NR 0
TC 0
Z9 0
U1 4
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 AUG 10
PY 2014
VL 248
MA 617-PMSE
PG 1
WC Chemistry, Multidisciplinary
SC Chemistry
GA CA8KC
UT WOS:000349167405103
ER
PT J
AU Meador, MA
AF Meador, Michael A.
TI Opportunities and challenges in nanomanufacturing for aerospace
applications
SO ABSTRACTS OF PAPERS OF THE AMERICAN CHEMICAL SOCIETY
LA English
DT Meeting Abstract
CT 248th National Meeting of the American-Chemical-Society (ACS)
CY AUG 10-14, 2014
CL San Francisco, CA
SP Amer Chem Soc
C1 [Meador, Michael A.] NASA, Struct & Mat Div, Glenn Res Ctr, Cleveland, OH 44135 USA.
EM Michael.A.Meador@nasa.gov
NR 0
TC 0
Z9 0
U1 1
U2 2
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 AUG 10
PY 2014
VL 248
MA 32-POLY
PG 1
WC Chemistry, Multidisciplinary
SC Chemistry
GA CA8KC
UT WOS:000349167405168
ER
PT J
AU Mertens, LA
Okumura, M
Sander, SP
AF Mertens, Laura A.
Okumura, Mitchio
Sander, Stanley P.
TI Temperature dependent branching ratios of HONO2 and HOONO from HOx and
NOx cross reactions found using pulsed cavity-ringdown spectroscopy
SO ABSTRACTS OF PAPERS OF THE AMERICAN CHEMICAL SOCIETY
LA English
DT Meeting Abstract
CT 248th National Meeting of the American-Chemical-Society (ACS)
CY AUG 10-14, 2014
CL San Francisco, CA
SP Amer Chem Soc
C1 [Mertens, Laura A.; Okumura, Mitchio] CALTECH, Pasadena, CA 91125 USA.
[Sander, Stanley P.] NASA, Jet Prop Lab, Pasadena, CA 91125 USA.
EM lmertens@caltech.edu
NR 0
TC 0
Z9 0
U1 2
U2 5
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 AUG 10
PY 2014
VL 248
MA 468-PHYS
PG 1
WC Chemistry, Multidisciplinary
SC Chemistry
GA CA8KC
UT WOS:000349167404186
ER
PT J
AU Monk, J
Lawson, JW
Haskins, J
Bauschlicher, C
AF Monk, Joshua
Lawson, John W.
Haskins, Justin
Bauschlicher, Charles
TI Thermal and mechanical properties of cross-linked phenolic resins for
thermal protection materials for space vehicles
SO ABSTRACTS OF PAPERS OF THE AMERICAN CHEMICAL SOCIETY
LA English
DT Meeting Abstract
CT 248th National Meeting of the American-Chemical-Society (ACS)
CY AUG 10-14, 2014
CL San Francisco, CA
SP Amer Chem Soc
C1 [Monk, Joshua; Lawson, John W.; Haskins, Justin] NASA, Ames Res Ctr, Thermal Protect Mat Branch, Moffett Field, CA 94035 USA.
[Bauschlicher, Charles] NASA, Ames Res Ctr, Entry Syst & Technol Div, Moffett Field, CA 94035 USA.
EM joshua.d.monk@nasa.gov
NR 0
TC 0
Z9 0
U1 1
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 AUG 10
PY 2014
VL 248
MA 477-COMP
PG 1
WC Chemistry, Multidisciplinary
SC Chemistry
GA CA8JN
UT WOS:000349165104680
ER
PT J
AU Parker, DSN
Yang, T
Kaiser, RI
Troy, T
Ahmed, M
Lee, TJ
AF Parker, Dorian S. N.
Yang, Tao
Kaiser, Ralf I.
Troy, Tyler
Ahmed, Musa
Lee, Timothy J.
TI On the formation of quinoline and the role of gas phase reactions in the
synthesis of prebiotic molecules
SO ABSTRACTS OF PAPERS OF THE AMERICAN CHEMICAL SOCIETY
LA English
DT Meeting Abstract
CT 248th National Meeting of the American-Chemical-Society (ACS)
CY AUG 10-14, 2014
CL San Francisco, CA
SP Amer Chem Soc
C1 [Parker, Dorian S. N.; Yang, Tao; Kaiser, Ralf I.] Univ Hawaii, Honolulu, HI 96816 USA.
[Troy, Tyler; Ahmed, Musa] Adv Light Source LBNL, Berkeley, CA 94720 USA.
[Lee, Timothy J.] NASA, Ames Res Ctr, Mountain View, CA USA.
EM dparker3@hawaii.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 AUG 10
PY 2014
VL 248
MA 107-PHYS
PG 1
WC Chemistry, Multidisciplinary
SC Chemistry
GA CA8KC
UT WOS:000349167403712
ER
PT J
AU Pickering, K
AF Pickering, Karen
TI Water: A critical material enabling space exploration
SO ABSTRACTS OF PAPERS OF THE AMERICAN CHEMICAL SOCIETY
LA English
DT Meeting Abstract
CT 248th National Meeting of the American-Chemical-Society (ACS)
CY AUG 10-14, 2014
CL San Francisco, CA
SP Amer Chem Soc
C1 [Pickering, Karen] NASA, Johnson Space Ctr, Dept Crew, Houston, TX 77058 USA.
[Pickering, Karen] NASA, Johnson Space Ctr, Thermal Syst Div, Houston, TX 77058 USA.
EM karen.d.pickering@nasa.gov
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 AUG 10
PY 2014
VL 248
MA 155-ANYL
PG 1
WC Chemistry, Multidisciplinary
SC Chemistry
GA CA8JN
UT WOS:000349165101604
ER
PT J
AU Rothschild, LJ
Fujishima, K
Paulino-LIma, I
AF Rothschild, Lynn J.
Fujishima, Kosuke
Paulino-LIma, Ivan
TI Synthetic biology and the search for extraterrestrial life
SO ABSTRACTS OF PAPERS OF THE AMERICAN CHEMICAL SOCIETY
LA English
DT Meeting Abstract
CT 248th National Meeting of the American-Chemical-Society (ACS)
CY AUG 10-14, 2014
CL San Francisco, CA
SP Amer Chem Soc
C1 [Rothschild, Lynn J.] NASA, Ames Res Ctr, Div Earth Sci, Moffett Field, CA 94035 USA.
[Fujishima, Kosuke] Univ Calif Santa Cruz, Univ Affiliated Res Ctr, NASA Ames Res Ctr, Div Earth Sci, Moffett Field, CA 94035 USA.
[Paulino-LIma, Ivan] NASA, Ames Res Ctr, NPP, Div Earth Sci, Moffett Field, CA 94035 USA.
EM Lynn.J.Rothschild@nasa.gov
NR 0
TC 0
Z9 0
U1 1
U2 9
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 AUG 10
PY 2014
VL 248
MA 50-PHYS
PG 1
WC Chemistry, Multidisciplinary
SC Chemistry
GA CA8KC
UT WOS:000349167403656
ER
PT J
AU Schwenke, DW
AF Schwenke, David W.
TI Handy's harbinger
SO ABSTRACTS OF PAPERS OF THE AMERICAN CHEMICAL SOCIETY
LA English
DT Meeting Abstract
CT 248th National Meeting of the American-Chemical-Society (ACS)
CY AUG 10-14, 2014
CL San Francisco, CA
SP Amer Chem Soc
C1 [Schwenke, David W.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
EM david.w.schwenke@nasa.gov
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 AUG 10
PY 2014
VL 248
MA 474-COMP
PG 1
WC Chemistry, Multidisciplinary
SC Chemistry
GA CA8JN
UT WOS:000349165104677
ER
PT J
AU Scott, VJ
Manohara, H
Toda, R
Murthy, R
Del Castillo, L
AF Scott, Valerie J.
Manohara, Harish
Toda, Risaku
Murthy, Rakesh
Del Castillo, Linda
TI Robust CNT field emitters: Growth and in situ welding on metal surfaces
SO ABSTRACTS OF PAPERS OF THE AMERICAN CHEMICAL SOCIETY
LA English
DT Meeting Abstract
CT 248th National Meeting of the American-Chemical-Society (ACS)
CY AUG 10-14, 2014
CL San Francisco, CA
SP Amer Chem Soc
C1 [Scott, Valerie J.; Manohara, Harish; Toda, Risaku; Murthy, Rakesh; Del Castillo, Linda] CALTECH, Jet Prop Lab, Pasadena, CA 91108 USA.
EM valerie.j.scott@jpl.nasa.gov
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 AUG 10
PY 2014
VL 248
MA 98-IEC
PG 1
WC Chemistry, Multidisciplinary
SC Chemistry
GA CA8KC
UT WOS:000349167400514
ER
PT J
AU Scott, VJ
Amashukeli, X
AF Scott, Valerie J.
Amashukeli, Xenia
TI RF-powered microreactor for efficient extraction and hydrolysis
SO ABSTRACTS OF PAPERS OF THE AMERICAN CHEMICAL SOCIETY
LA English
DT Meeting Abstract
CT 248th National Meeting of the American-Chemical-Society (ACS)
CY AUG 10-14, 2014
CL San Francisco, CA
SP Amer Chem Soc
C1 [Scott, Valerie J.; Amashukeli, Xenia] CALTECH, Jet Prop Lab, Pasadena, CA USA.
EM valerie.j.scott@jpl.nasa.gov
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 AUG 10
PY 2014
VL 248
MA 11-ANYL
PG 1
WC Chemistry, Multidisciplinary
SC Chemistry
GA CA8JN
UT WOS:000349165101469
ER
PT J
AU Simpson, WR
Peterson, PK
Nghiem, SV
AF Simpson, William R.
Peterson, Peter K.
Nghiem, Son V.
TI Vertical and horizontal gradients in bromine monoxide assist in
understanding arctic halogen activation mechanisms
SO ABSTRACTS OF PAPERS OF THE AMERICAN CHEMICAL SOCIETY
LA English
DT Meeting Abstract
CT 248th National Meeting of the American-Chemical-Society (ACS)
CY AUG 10-14, 2014
CL San Francisco, CA
SP Amer Chem Soc
C1 [Simpson, William R.; Peterson, Peter K.] Univ Alaska Fairbanks, Dept Chem & Biochem, Fairbanks, AK 99775 USA.
[Simpson, William R.; Peterson, Peter K.] Univ Alaska Fairbanks, Inst Geophys, Fairbanks, AK 99775 USA.
[Nghiem, Son V.] CALTECH, Radar Sci & Engn Sect, Jet Prop Lab, Pasadena, CA 91109 USA.
EM wrsimpson@alaska.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 AUG 10
PY 2014
VL 248
MA 92-PHYS
PG 1
WC Chemistry, Multidisciplinary
SC Chemistry
GA CA8KC
UT WOS:000349167403697
ER
PT J
AU Smith, KE
Callahan, MP
Gerakines, PA
Dworkin, JP
House, CH
AF Smith, Karen E.
Callahan, Michael P.
Gerakines, Perry A.
Dworkin, Jason P.
House, Christopher H.
TI Investigation of pyridine carboxylic acids in CM2 carbonaceous
chondrites: Potential precursor molecules for ancient coenzymes
SO ABSTRACTS OF PAPERS OF THE AMERICAN CHEMICAL SOCIETY
LA English
DT Meeting Abstract
CT 248th National Meeting of the American-Chemical-Society (ACS)
CY AUG 10-14, 2014
CL San Francisco, CA
SP Amer Chem Soc
C1 [Smith, Karen E.; House, Christopher H.] Penn State Univ, Dept Geosci, University Pk, PA 16802 USA.
[Smith, Karen E.; House, Christopher H.] Penn State Univ, Penn State Astrobiol Res Ctr, University Pk, PA 16802 USA.
[Smith, Karen E.] Oak Ridge Associated Univ, NASA Goddard Space Flight Ctr, Oak Ridge, TN 37831 USA.
[Callahan, Michael P.; Gerakines, Perry A.; Dworkin, Jason P.] NASA Goddard Space Flight Ctr, Solar Syst Explorat Div, Greenbelt, MD 20771 USA.
EM karen.e.smith@nasa.gov
RI Dworkin, Jason/C-9417-2012
OI Dworkin, Jason/0000-0002-3961-8997
NR 0
TC 0
Z9 0
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 AUG 10
PY 2014
VL 248
MA 120-ANYL
PG 1
WC Chemistry, Multidisciplinary
SC Chemistry
GA CA8JN
UT WOS:000349165101571
ER
PT J
AU Templeton, PD
Wagschal, K
Paavola, CD
Lee, CC
AF Templeton, Paul D.
Wagschal, Kurt
Paavola, Chad D.
Lee, Charles C.
TI Lignocellulose hydrolysis by multienzyme complexes
SO ABSTRACTS OF PAPERS OF THE AMERICAN CHEMICAL SOCIETY
LA English
DT Meeting Abstract
CT 248th National Meeting of the American-Chemical-Society (ACS)
CY AUG 10-14, 2014
CL San Francisco, CA
SP Amer Chem Soc
C1 [Templeton, Paul D.; Wagschal, Kurt; Lee, Charles C.] USDA ARS, Albany, CA 94710 USA.
[Paavola, Chad D.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
EM paul.templeton@ars.usda.gov
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 AUG 10
PY 2014
VL 248
MA 68-BIOL
PG 1
WC Chemistry, Multidisciplinary
SC Chemistry
GA CA8JN
UT WOS:000349165101875
ER
PT J
AU Vaidehi, N
Jain, A
Larsen, AB
Wagner, JE
Kandel, S
Salomon-Ferrer, R
AF Vaidehi, Nagarajan
Jain, Abhinandan
Larsen, Adrien B.
Wagner, Jeffrey E.
Kandel, Saugat
Salomon-Ferrer, Romelia
TI GNEIMO: An accurate internal coordinate molecular dynamics simulation
method for studying biomolecular dynamics
SO ABSTRACTS OF PAPERS OF THE AMERICAN CHEMICAL SOCIETY
LA English
DT Meeting Abstract
CT 248th National Meeting of the American-Chemical-Society (ACS)
CY AUG 10-14, 2014
CL San Francisco, CA
SP Amer Chem Soc
C1 [Vaidehi, Nagarajan; Larsen, Adrien B.; Wagner, Jeffrey E.; Kandel, Saugat; Salomon-Ferrer, Romelia] City Hope Natl Med Ctr, Beckman Res Inst, Dept Immunol, Duarte, CA 91010 USA.
[Jain, Abhinandan] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
EM nvaidehi@coh.org
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 AUG 10
PY 2014
VL 248
MA 70-COMP
PG 1
WC Chemistry, Multidisciplinary
SC Chemistry
GA CA8JN
UT WOS:000349165104312
ER
PT J
AU Wang, LM
Liu, YD
Campos-Pineda, M
Priest, C
Zhang, JS
AF Wang, Liming
Liu, Yingdi
Campos-Pineda, Mixtli
Priest, Chad
Zhang, Jingsong
TI Studying ozonolysis reactions of 2-butenes using cavity ring-down
spectroscopy
SO ABSTRACTS OF PAPERS OF THE AMERICAN CHEMICAL SOCIETY
LA English
DT Meeting Abstract
CT 248th National Meeting of the American-Chemical-Society (ACS)
CY AUG 10-14, 2014
CL San Francisco, CA
SP Amer Chem Soc
C1 [Wang, Liming] S China Univ Technol, Sch Chem & Chem Engn, Guangzhou 510640, Guangdong, Peoples R China.
[Liu, Yingdi] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Campos-Pineda, Mixtli; Priest, Chad; Zhang, Jingsong] Univ Calif Riverside, Riverside, CA 92521 USA.
EM yingdi@caltech.edu; jingsong.zhang@ucr.edu
NR 0
TC 0
Z9 0
U1 1
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 AUG 10
PY 2014
VL 248
MA 576-PHYS
PG 1
WC Chemistry, Multidisciplinary
SC Chemistry
GA CA8KC
UT WOS:000349167404282
ER
PT J
AU Williams, JC
Meador, MAB
AF Williams, Jarrod C.
Meador, Mary Ann B.
TI Synthesis and properties of porous polyamide aerogels with flexible
aliphatic segments
SO ABSTRACTS OF PAPERS OF THE AMERICAN CHEMICAL SOCIETY
LA English
DT Meeting Abstract
CT 248th National Meeting of the American-Chemical-Society (ACS)
CY AUG 10-14, 2014
CL San Francisco, CA
SP Amer Chem Soc
C1 [Williams, Jarrod C.; Meador, Mary Ann B.] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA.
EM jcwilli1@kent.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 AUG 10
PY 2014
VL 248
MA 623-PMSE
PG 1
WC Chemistry, Multidisciplinary
SC Chemistry
GA CA8KC
UT WOS:000349167405109
ER
PT J
AU Gatebe, C
Kuznetsov, A
Melnikova, I
AF Gatebe, C.
Kuznetsov, A.
Melnikova, I.
TI Cloud optical parameters from airborne observation of diffuse solar
radiation accomplished in USA and USSR in different geographical regions
SO INTERNATIONAL JOURNAL OF REMOTE SENSING
LA English
DT Article
ID SPECTRAL MEASUREMENTS; ATMOSPHERE; OZONE; VARIABILITY; ECOSYSTEMS;
ABSORPTION
AB Cloud optical parameters (optical thickness, single scattering albedo, and ground albedo) are obtained from airborne experiments with NASA's Cloud Absorption Radiometer and analysed taking into account observational and processing uncertainties. The analytical approach of the inverse asymptotic formulas of the transfer theory, which uses observed values of solar diffuse radiance, is applied. The method is free from a priori restrictions and links put to desired parameters. The algorithms and first results of processing have been presented earlier. The first results, being the solution of the inverse problem, showed strong fluctuations in values, which required the regularization of the solution. The dependence of uncertainties of the result on viewing direction was revealed. Hence, here attention is focused on uncertainties of observation, angle function calculation, and processing approach, which is taken into account for result averaging, and the regularization procedure is described. Calculating the uncertainties of the processing approach is accomplished analytically using formulas for the retrieval of the optical parameters. The values of the desired parameters obtained in eight observational spectral channels above, below, and within the cloud - at 16 levels are presented. The final results are compared to the optical parameters of extended cloud layers obtained earlier using a similar method of inverse asymptotic formulas from spectral data of Russian aircraft solar irradiance measurements in different regions, made in the 1970s/1980s at Leningrad (now Saint Petersburg) University in the USSR.
C1 [Gatebe, C.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Kuznetsov, A.; Melnikova, I.] Russian State Hydrometeorol Univ, Atmospher Phys Dept, St Petersburg, Russia.
RP Melnikova, I (reprint author), Russian State Hydrometeorol Univ, Atmospher Phys Dept, St Petersburg, Russia.
EM irina.melnikova@pobox.spbu.ru
RI Gatebe, Charles/G-7094-2011
OI Gatebe, Charles/0000-0001-9261-2239
NR 37
TC 3
Z9 4
U1 2
U2 4
PU TAYLOR & FRANCIS LTD
PI ABINGDON
PA 4 PARK SQUARE, MILTON PARK, ABINGDON OX14 4RN, OXON, ENGLAND
SN 0143-1161
EI 1366-5901
J9 INT J REMOTE SENS
JI Int. J. Remote Sens.
PD AUG 10
PY 2014
VL 35
IS 15
SI SI
BP 5812
EP 5829
DI 10.1080/01431161.2014.945000
PG 18
WC Remote Sensing; Imaging Science & Photographic Technology
SC Remote Sensing; Imaging Science & Photographic Technology
GA AO8WU
UT WOS:000341637000016
ER
PT J
AU Snowden, SL
Chiao, M
Collier, MR
Porter, FS
Thomas, NE
Cravens, T
Robertson, IP
Galeazzi, M
Uprety, Y
Ursino, E
Koutroumpa, D
Kuntz, KD
Lallement, R
Puspitarini, L
Lepri, ST
McCammon, D
Morgan, K
Walsh, BM
AF Snowden, S. L.
Chiao, M.
Collier, M. R.
Porter, F. S.
Thomas, N. E.
Cravens, T.
Robertson, I. P.
Galeazzi, M.
Uprety, Y.
Ursino, E.
Koutroumpa, D.
Kuntz, K. D.
Lallement, R.
Puspitarini, L.
Lepri, S. T.
McCammon, D.
Morgan, K.
Walsh, B. M.
TI PRESSURE EQUILIBRIUM BETWEEN THE LOCAL INTERSTELLAR CLOUDS AND THE LOCAL
HOT BUBBLE
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE ISM: bubbles; ISM: clouds; magnetic fields; solar neighborhood; X-rays:
diffuse background; X-rays: ISM
ID X-RAY-EMISSION; EXTREME-ULTRAVIOLET EMISSION; MAPS; GAS; SOLAR; ISM;
ABUNDANCES; IONS; LINE; SUN
AB Three recent results related to the heliosphere and the local interstellar medium (ISM) have provided an improved insight into the distribution and conditions of material in the solar neighborhood. These are the measurement of the magnetic field outside of the heliosphere by Voyager 1, the improved mapping of the three-dimensional structure of neutral material surrounding the Local Cavity using extensive ISM absorption line and reddening data, and a sounding rocket flight which observed the heliospheric helium focusing cone in X-rays and provided a robust estimate of the contribution of solar wind charge exchange emission to the ROSAT All-Sky Survey 1/4 keV band data. Combining these disparate results, we show that the thermal pressure of the plasma in the Local Hot Bubble (LHB) is P/k = 10,700 cm(-3) K. If the LHB is relatively free of a global magnetic field, it can easily be in pressure (thermal plus magnetic field) equilibrium with the local interstellar clouds, eliminating a long-standing discrepancy in models of the local ISM.
C1 [Snowden, S. L.; Chiao, M.; Collier, M. R.; Porter, F. S.; Thomas, N. E.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Cravens, T.; Robertson, I. P.] Univ Kansas, Dept Phys & Astron, Lawrence, KS 66045 USA.
[Galeazzi, M.; Uprety, Y.; Ursino, E.] Univ Miami, Dept Phys, Coral Gables, FL 33146 USA.
[Koutroumpa, D.] Univ Paris 06, Sorbonne Univ, Univ Versailles St Quentin, CNRS INSU,LATMOS IPSL, F-78280 Guyancourt, France.
[Kuntz, K. D.] Johns Hopkins Univ, Henry A Rowland Dept Phys & Astron, Baltimore, MD 21218 USA.
[Lallement, R.; Puspitarini, L.] Univ Paris Diderot, CNRS UMR8111, Observ Paris, GEPI, F-92190 Meudon, France.
[Lepri, S. T.] Univ Michigan, Ann Arbor, MI 48109 USA.
[McCammon, D.; Morgan, K.] Univ Wisconsin, Dept Phys, Madison, WI 53706 USA.
[Walsh, B. M.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
RP Snowden, SL (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
EM steven.l.snowden@nasa.gov
RI Porter, Frederick/D-3501-2012; Morgan, Kelsey/J-5053-2016; Collier,
Michael/I-4864-2013
OI Porter, Frederick/0000-0002-6374-1119; Morgan,
Kelsey/0000-0002-6597-1030; Collier, Michael/0000-0001-9658-6605
FU NASA's award [NNX11AF04G]
FX We are grateful to Ed Jenkins for interesting and helpful insights into
these results. This work has been supported in part by NASA's award
#NNX11AF04G.
NR 33
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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
EI 2041-8213
J9 ASTROPHYS J LETT
JI Astrophys. J. Lett.
PD AUG 10
PY 2014
VL 791
IS 1
AR L14
DI 10.1088/2041-8205/791/1/L14
PG 3
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AO4JB
UT WOS:000341302200015
ER
PT J
AU Walsh, C
Juhasz, A
Pinilla, P
Harsono, D
Mathews, GS
Dent, WRF
Hogerheijde, MR
Birnstiel, T
Meeus, G
Nomura, H
Aikawa, Y
Millar, TJ
Sandell, G
AF Walsh, Catherine
Juhasz, Attila
Pinilla, Paola
Harsono, Daniel
Mathews, Geoffrey S.
Dent, William R. F.
Hogerheijde, Michiel R.
Birnstiel, T.
Meeus, Gwendolyn
Nomura, Hideko
Aikawa, Yuri
Millar, T. J.
Sandell, Goeran
TI ALMA HINTS AT THE PRESENCE OF TWO COMPANIONS IN THE DISK AROUND HD
100546
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE protoplanetary disks; stars: formation; stars: individual (HD 100546);
stars: pre-main sequence; submillimeter: planetary systems
ID HERBIG AE/BE STARS; NEAR-INFRARED SPECTROSCOPY; CO EMISSION-LINES;
PROTOPLANETARY DISKS; DIGIT SURVEY; TW-HYDRAE; WARM GAS; DUST;
HD-100546; PLANET
AB HD 100546 is a well-studied Herbig Be star-disk system that likely hosts a close-in companion with compelling observational evidence for an embedded protoplanet at 68 AU. We present Atacama Large Millimeter/Submillimeter Array observations of the HD 100546 disk which resolve the gas and dust structure at (sub) millimeter wavelengths. The CO emission (at 345.795 GHz) originates from an extensive molecular disk (390 +/- 20 AU in radius) whereas the continuum emission is more compact (230 +/- 20 AU in radius), suggesting radial drift of the millimeter-sized grains. The CO emission is similar in extent to scattered light images indicating well-mixed gas and micrometer-sized grains in the disk atmosphere. Assuming azimuthal symmetry, a single-component power-law model cannot reproduce the continuum visibilities. The visibilities and images are better reproduced by a double-component model: a compact ring with a width of 21 AU centered at 26 AU and an outer ring with a width of 75 +/- 3 AU centered at 190 +/- 3 AU. The influence of a companion and protoplanet on the dust evolution is investigated. The companion at 10 AU facilitates the accumulation of millimeter-sized grains within a compact ring, approximate to 20-30 AU, by approximate to 10 Myr. The injection of a protoplanet at 1 Myr hastens the ring formation (approximate to 1.2 Myr) and also triggers the development of an outer ring (approximate to 100-200 AU). These observations provide additional evidence for the presence of a close-in companion and hint at dynamical clearing by a protoplanet in the outer disk.
C1 [Walsh, Catherine; Juhasz, Attila; Pinilla, Paola; Harsono, Daniel; Mathews, Geoffrey S.; Hogerheijde, Michiel R.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands.
[Harsono, Daniel] SRON Netherlands Inst Space Res, SRON, NL-9700 AV Groningen, Netherlands.
[Mathews, Geoffrey S.] Univ Hawaii, Dept Phys & Astron, Honolulu, HI 96822 USA.
[Dent, William R. F.] Joint ALMA Observ JAO, Santiago, Chile.
[Dent, William R. F.] European So Observ, Santiago 19, Chile.
[Birnstiel, T.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Meeus, Gwendolyn] Univ Autonoma Madrid, Fac Ciencias, Dept Fis Teor, E-28049 Madrid, Spain.
[Nomura, Hideko] Tokyo Inst Technol, Dept Earth & Planetary Sci, Meguro Ku, Tokyo 1528551, Japan.
[Aikawa, Yuri] Kobe Univ, Dept Earth & Planetary Sci, Nada Ku, Kobe, Hyogo 6578501, Japan.
[Millar, T. J.] Queens Univ Belfast, Sch Math & Phys, Astrophys Res Ctr, Belfast BT7 1NN, Antrim, North Ireland.
[Sandell, Goeran] NASA, Ames Res Ctr, SOFIA USRA, Moffett Field, CA 94035 USA.
RP Walsh, C (reprint author), Leiden Univ, Leiden Observ, POB 9513, NL-2300 RA Leiden, Netherlands.
OI Millar, Tom/0000-0001-5178-3656; Hogerheijde,
Michiel/0000-0001-5217-537X; Birnstiel, Tilman/0000-0002-1899-8783
FU Netherlands Organisation for Scientific Research (NWO) [639.041.335]; EU
A-ERC [291141]; KNAW; NASA Origins of Solar Systems [NNX12AJ04G]; STFC;
Netherlands Organization for Scientific Research (NWO); European ALMA
Regional Center node in the Netherlands
FX This Letter makes use of the following ALMA data:
ADS/JAO.ALMA#2011.0.00863. 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. The authors thank E. F. van Dishoeck, C. P. Dullemond, N. van der
Marel, and M. Schmalzl for useful discussions, and G. D. Mulders for
sharing the results of his hydrodynamical simulations. C. W.
acknowledges support from the Netherlands Organisation for Scientific
Research (NWO, program number 639.041.335). This work was also supported
by EU A-ERC grant 291141 CHEMPLAN and a KNAW prize. T. B. acknowledges
support from NASA Origins of Solar Systems grant NNX12AJ04G.
Astrophysics at QUB is supported by a grant from the STFC. M. R. H., A.
J., and G. S. M. acknowledge support from the Netherlands Organization
for Scientific Research (NWO) to Allegro, the European ALMA Regional
Center node in the Netherlands.
NR 44
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U1 1
U2 4
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 AUG 10
PY 2014
VL 791
IS 1
AR L6
DI 10.1088/2041-8205/791/1/L6
PG 6
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AO4JB
UT WOS:000341302200006
ER
PT J
AU Bodaghee, A
Tomsick, JA
Krivonos, R
Stern, D
Bauer, FE
Fornasini, FM
Barriere, N
Boggs, SE
Christensen, FE
Craig, WW
Gotthelf, EV
Hailey, CJ
Harrison, FA
Hong, J
Mori, K
Zhang, WW
AF Bodaghee, Arash
Tomsick, John A.
Krivonos, Roman
Stern, Daniel
Bauer, Franz E.
Fornasini, Francesca M.
Barriere, Nicolas
Boggs, Steven E.
Christensen, Finn E.
Craig, William W.
Gotthelf, Eric V.
Hailey, Charles J.
Harrison, Fiona A.
Hong, Jaesub
Mori, Kaya
Zhang, William W.
TI INITIAL RESULTS FROM NuSTAR OBSERVATIONS OF THE NORMA ARM
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE binaries: general; novae, cataclysmic variables; stars: neutron; X-rays:
binaries
ID MAGNETIC CATACLYSMIC VARIABLES; X-RAY SURVEY; GALACTIC-CENTER;
STAR-FORMATION; CATALOG; COMPLEX
AB Results are presented for an initial survey of the Norma Arm gathered with the focusing hard X-Ray Telescope NuSTAR. The survey covers 0.2 deg(2) of sky area in the 3-79 keV range with a minimum and maximum raw depth of 15 ks and 135 ks, respectively. Besides a bright black-hole X-ray binary in outburst (4U 1630-47) and a new X-ray transient (NuSTAR J163433-473841), NuSTAR locates three sources from the Chandra survey of this region whose spectra are extended above 10 keV for the first time: CXOU J163329.5-473332, CXOU J163350.9-474638, and CXOU J163355.1-473804. Imaging, timing, and spectral data from a broad X-ray range (0.3-79 keV) are analyzed and interpreted with the aim of classifying these objects. CXOU J163329.5-473332 is either a cataclysmic variable or a faint low-mass X-ray binary. CXOU J163350.9-474638 varies in intensity on year-long timescales, and with no multi-wavelength counterpart, it could be a distant X-ray binary or possibly a magnetar. CXOU J163355.1-473804 features a helium-like iron line at 6.7 keV and is classified as a nearby cataclysmic variable. Additional surveys are planned for the Norma Arm and Galactic Center, and those NuSTAR observations will benefit from the lessons learned during this pilot study.
C1 [Bodaghee, Arash; Tomsick, John A.; Krivonos, Roman; Barriere, Nicolas; Boggs, Steven E.; Craig, William W.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
[Bodaghee, Arash] Georgia Coll & State Univ, Milledgeville, GA 31061 USA.
[Stern, Daniel] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Bauer, Franz E.] Pontificia Univ Catolica Chile, Fac Fis, Inst Astrofis, Santiago 22, Chile.
[Bauer, Franz E.] Millennium Inst Astrophys, Santiago, Chile.
[Bauer, Franz E.] Space Sci Inst, Boulder, CO 80301 USA.
[Fornasini, Francesca M.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA.
[Christensen, Finn E.] Tech Univ Denmark, DTU Space, Natl Space Inst, DK-2800 Lyngby, Denmark.
[Craig, William W.] Lawrence Livermore Natl Lab, Livermore, CA 94550 USA.
[Gotthelf, Eric V.; Hailey, Charles J.; Mori, Kaya] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA.
[Harrison, Fiona A.] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA.
[Hong, Jaesub] Harvard Univ, Dept Astron, Cambridge, MA 02138 USA.
[Zhang, William W.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Bodaghee, A (reprint author), Univ Calif Berkeley, Space Sci Lab, 7 Gauss Way, Berkeley, CA 94720 USA.
RI Boggs, Steven/E-4170-2015
OI Boggs, Steven/0000-0001-9567-4224
FU NASA [NNG08FD60C]; National Science Foundation Graduate Research
Fellowship; BasalCATA [PFB-06/2007]; CONICYT-Chile [FONDECYT 1141218]
FX This work was supported under NASA Contract No. NNG08FD60C, and made use
of data from the NuSTAR mission, a project led by the California
Institute of Technology, managed by the Jet Propulsion Laboratory, and
funded by the National Aeronautics and Space Administration. We thank
the NuSTAR Operations, Software, and Calibration teams for support with
the execution and analysis of these observations. This research has made
use of the NuSTAR Data Analysis Software (NuSTAR-DAS) jointly developed
by the ASI Science Data Center (ASDC, Italy) and the California
Institute of Technology. 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; NASA's
Astrophysics Data System Bibliographic Services; and the SIMBAD database
operated at CDS, Strasbourg, France. F. M. F. acknowledges support from
the National Science Foundation Graduate Research Fellowship. F. E. B.
acknowledges support from BasalCATA PFB-06/2007, CONICYT-Chile (FONDECYT
1141218 and "EMBIGGEN" Anillo ACT1101), and Project IC120009 "Millennium
Institute of Astrophysics (MAS)" of Iniciativa Cient ' ifica Milenio del
Ministerio de Economia, Fomento y Turismo.
NR 37
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U1 1
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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 AUG 10
PY 2014
VL 791
IS 1
AR 68
DI 10.1088/0004-637X/791/1
PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AM2CY
UT WOS:000339657700068
ER
PT J
AU Bond, NA
Gardner, JP
de Mello, DF
Teplitz, HI
Rafelski, M
Koekemoer, AM
Coe, D
Grogin, N
Gawiser, E
Ravindranath, S
Scarlata, C
AF Bond, Nicholas A.
Gardner, Jonathan P.
de Mello, Duilia F.
Teplitz, Harry I.
Rafelski, Marc
Koekemoer, Anton M.
Coe, Dan
Grogin, Norman
Gawiser, Eric
Ravindranath, Swara
Scarlata, Claudia
TI THE REST-FRAME ULTRAVIOLET STRUCTURE OF 0.5 < z < 1.5 GALAXIES
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE cosmology: observations; galaxies: formation; galaxies: high-redshift;
galaxies: structure
ID STAR-FORMING GALAXIES; ULTRA DEEP FIELD; GOODS-SOUTH FIELD; SIMILAR-TO
2; EXTRAGALACTIC LEGACY SURVEY; HIGH-REDSHIFT; VLT/FORS2 SPECTROSCOPY;
ADVANCED CAMERA; CLUMP-CLUSTER; PART II
AB We present the rest-frame UV wavelength dependence of the Petrosian-like half-light radius (r(50)), and the concentration parameter for a sample of 198 star-forming galaxies at 0.5 < z < 1.5. We find a similar to 5% decrease in r(50) from 1500 angstrom to 3000 angstrom, with half-light radii at 3000 ranging from 0.6 kpc to 6 kpc. We also find a decrease in concentration of similar to 0.07 (1.9 < C-3000 < 3.9). The lack of a strong relationship between r(50) and wavelength is consistent with a model in which clumpy star formation is distributed over length scales comparable to the galaxy's rest-frame optical light. While the wavelength dependence of r50 is independent of size at all redshifts, concentration decreases more sharply in the far-UV (similar to 1500 angstrom) for large galaxies at z similar to 1. This decrease in concentration is caused by a flattening of the inner similar to 20% of the light profile in disk-like galaxies, indicating that the central regions have different UV colors than the rest of the galaxy. We interpret this as a bulge component with older stellar populations and/or more dust. The size-dependent decrease in concentration is less dramatic at z similar to 2, suggesting that bulges are less dusty, younger, and/or less massive than the rest of the galaxy at higher redshifts.
C1 [Bond, Nicholas A.; Gardner, Jonathan P.] NASA, Goddard Space Flight Ctr, Cosmol Lab, Greenbelt, MD 20771 USA.
[de Mello, Duilia F.] Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA.
[Teplitz, Harry I.; Rafelski, Marc] CALTECH, IPAC, Pasadena, CA 91125 USA.
[Koekemoer, Anton M.; Coe, Dan; Grogin, Norman] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
[Gawiser, Eric] Rutgers State Univ, Dept Phys & Astron, Piscataway, NJ 08854 USA.
[Ravindranath, Swara] Interuniv Ctr Astron & Astrophys, Pune, Maharashtra, India.
[Scarlata, Claudia] Univ Minnesota, Sch Phys & Astron, Minnesota Inst Astrophys, Minneapolis, MN 55455 USA.
RP Bond, NA (reprint author), NASA, Goddard Space Flight Ctr, Cosmol Lab, Code 665, Greenbelt, MD 20771 USA.
OI Gawiser, Eric/0000-0003-1530-8713; Koekemoer, Anton/0000-0002-6610-2048
FU Space Telescope Science Institute [HST-GO-12534]; Association of
Universities for Research in Astronomy, Inc., under NASA [NAS 5-26555]
FX Support for program number HST-GO-12534 was provided by NASA through a
grant 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.
NR 48
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U1 0
U2 0
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 AUG 10
PY 2014
VL 791
IS 1
AR 18
DI 10.1088/0004-637X/791/1/18
PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AM2CY
UT WOS:000339657700018
ER
PT J
AU Klimchuk, JA
Bradshaw, SJ
AF Klimchuk, J. A.
Bradshaw, S. J.
TI ARE CHROMOSPHERIC NANOFLARES A PRIMARY SOURCE OF CORONAL PLASMA?
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE Sun: chromosphere; Sun: corona; Sun: UV radiation
ID IMAGING SPECTROMETER OBSERVATIONS; ACTIVE-REGION LOOPS; DOPPLER SHIFTS;
SPECTROSCOPIC OBSERVATIONS; TRANSITION REGION; TIME-DEPENDENCE; SOLAR
CORONA; QUIET SUN; EMISSION; CORE
AB It has been suggested that the hot plasma of the solar corona comes primarily from impulsive heating events, or nanoflares, that occur in the lower atmosphere, either in the upper part of the ordinary chromosphere or at the tips of type II spicules. We test this idea with a series of hydrodynamic simulations. We find that synthetic Fe XII (195) and Fe XIV (274) line profiles generated from the simulations disagree dramatically with actual observations. The integrated line intensities are much too faint; the blueshifts are much too fast; the blue-red asymmetries are much too large; and the emission is confined to low altitudes. We conclude that chromospheric nanoflares are not a primary source of hot coronal plasma. Such events may play an important role in producing the chromosphere and powering its intense radiation, but they do not, in general, raise the temperature of the plasma to coronal values. Those cases where coronal temperatures are reached must be relatively uncommon. The observed profiles of Fe XII and Fe XIV come primarily from plasma that is heated in the corona itself, either by coronal nanoflares or a quasi-steady coronal heating process. Chromospheric nanoflares might play a role in generating waves that provide this coronal heating.
C1 [Klimchuk, J. A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Bradshaw, S. J.] Rice Univ, Dept Phys & Astron, Houston, TX 77005 USA.
RP Klimchuk, JA (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
EM James.A.Klimchuk@nasa.gov; stephen.bradshaw@rice.edu
RI Klimchuk, James/D-1041-2012
OI Klimchuk, James/0000-0003-2255-0305
FU NASA Supporting Research and Technology Program
FX This work was supported by the NASA Supporting Research and Technology
Program. The authors benefited from participation in the International
Space Science Institute team on Using Observables to Settle the Question
of Steady versus Impulsive Coronal Heating, led by one of us (S.J.B.)
and Helen Mason.
NR 34
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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 AUG 10
PY 2014
VL 791
IS 1
AR 60
DI 10.1088/0004-637X/791/1/60
PG 7
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AM2CY
UT WOS:000339657700060
ER
PT J
AU Kushwaha, U
Joshi, B
Cho, KS
Veronig, A
Tiwari, SK
Mathew, SK
AF Kushwaha, Upendra
Joshi, Bhuwan
Cho, Kyung-Suk
Veronig, Astrid
Tiwari, Sanjiv Kumar
Mathew, S. K.
TI IMPULSIVE ENERGY RELEASE AND NON-THERMAL EMISSION IN A CONFINED M4.0
FLARE TRIGGERED BY RAPIDLY EVOLVING MAGNETIC STRUCTURES
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE Sun: corona; Sun: flares; Sun: X-rays, gamma rays
ID CORONAL MASS EJECTIONS; DOUBLE-LOOP CONFIGURATION; X-RAY TELESCOPE;
SOLAR-FLARES; EXTREME-ULTRAVIOLET; FLUX EMERGENCE; RECONNECTION; FIELD;
ERUPTIONS; RHESSI
AB We present observations of a confined M4.0 flare from NOAA 11302 on 2011 September 26. Observations at high temporal, spatial, and spectral resolution from the Solar Dynamics Observatory, Reuven Ramaty High Energy Solar Spectroscopic Imager, and Nobeyama Radioheliograph observations enabled us to explore the possible triggering and energy release processes of this flare despite its very impulsive behavior and compact morphology. The flare light curves exhibit an abrupt rise of non-thermal emission with co-temporal hard X-ray (HXR) and microwave (MW) bursts that peaked instantly without any precursor emission. This stage was associated with HXR emission up to 200 keV that followed a power law with photon spectral index (gamma) similar to 3. Another non-thermal peak, observed 32 s later, was more pronounced in the MW flux than the HXR profiles. Dual peaked structures in the MW and HXR light curves suggest a two-step magnetic reconnection process. Extreme ultraviolet (EUV) images exhibit a sequential evolution of the inner and outer core regions of magnetic loop systems while the overlying loop configuration remained unaltered. Combined observations in HXR, (E) UV, and Ha provide support for flare models involving the interaction of coronal loops. The magnetograms obtained by the Helioseismic and Magnetic Imager reveal emergence of magnetic flux that began similar to five hr before the flare. However, the more crucial changes in the photospheric magnetic flux occurred about one minute prior to the flare onset with opposite polarity magnetic transients appearing at the early flare location within the inner core region. The spectral, temporal, and spatial properties of magnetic transients suggest that the sudden changes in the small-scale magnetic field have likely triggered the flare by destabilizing the highly sheared pre-flare magnetic configuration.
C1 [Kushwaha, Upendra; Joshi, Bhuwan; Mathew, S. K.] Udaipur Solar Observ, Phys Res Lab, Udaipur 313001, India.
[Cho, Kyung-Suk] Korea Astron & Space Sci Inst, Taejon 305348, South Korea.
[Veronig, Astrid] Graz Univ, Inst Phys, Kanzelhohe Observ, A-8010 Graz, Austria.
[Tiwari, Sanjiv Kumar] NASA, Marshall Space Flight Ctr, Huntsville, AL 35812 USA.
RP Kushwaha, U (reprint author), Udaipur Solar Observ, Phys Res Lab, Udaipur 313001, India.
EM upendra@prl.res.in
RI Veronig, Astrid/B-8422-2009;
OI Kushwaha, Upendra/0000-0001-6750-4578
FU "Development of Korea SpaceWeather Center" of KASI; KASI basic research
funds; Austrian Science Fund (FWF) [P24092-N16]; NASA Postdoctoral
Program at the NASAMarshall Space Flight Center
FX We thank theSDO, RHESSI, NoRH, andGOESteams for their open data policy.
SDO and RHESSI are NASA's missions under living with a star and small
explorer programs, respectively. We are grateful to S. Couvidat of
Stanford University for providing the SDO/HMI spectral data. We express
our sincere gratitude to P. Venkatakrishnan (USO/PRL), Jongchul Chae
(Seoul National University), and Yong-JaeMoon (Kyung-Hee University) for
useful discussions. K. S. C. is supported by the "Development of Korea
SpaceWeather Center" of KASI and the KASI basic research funds. A. V.
gratefully acknowledges the Austrian Science Fund (FWF): P24092-N16. S.
K. T. is supported by an appointment to the NASA Postdoctoral Program at
the NASAMarshall Space Flight Center, administered by Oak Ridge
Associated Universities through a contract with NASA. We sincerely thank
the anonymous referee for providing constructive comments and
suggestions that have enhanced the quality and presentation of this
paper.
NR 46
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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 AUG 10
PY 2014
VL 791
IS 1
AR 23
DI 10.1088/0004-637X/791/1/23
PG 16
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AM2CY
UT WOS:000339657700023
ER
PT J
AU Maseda, MV
van der Wel, A
Rix, HW
da Cunha, E
Pacifici, C
Momcheva, I
Brammer, GB
Meidt, SE
Franx, M
van Dokkum, P
Fumagalli, M
Bell, EF
Ferguson, HC
Forster-Schreiber, NM
Koekemoer, AM
Koo, DC
Lundgren, BF
Marchesini, D
Nelson, EJ
Patel, SG
Skelton, RE
Straughn, AN
Trump, JR
Whitaker, KE
AF Maseda, Michael V.
van der Wel, Arjen
Rix, Hans-Walter
da Cunha, Elisabete
Pacifici, Camilla
Momcheva, Ivelina
Brammer, Gabriel B.
Meidt, Sharon E.
Franx, Marijn
van Dokkum, Pieter
Fumagalli, Mattia
Bell, Eric F.
Ferguson, Henry C.
Foerster-Schreiber, Natascha M.
Koekemoer, Anton M.
Koo, David C.
Lundgren, Britt F.
Marchesini, Danilo
Nelson, Erica J.
Patel, Shannon G.
Skelton, Rosalind E.
Straughn, Amber N.
Trump, Jonathan R.
Whitaker, Katherine E.
TI THE NATURE OF EXTREME EMISSION LINE GALAXIES AT z=1-2: KINEMATICS AND
METALLICITIES FROM NEAR-INFRARED SPECTROSCOPY
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: dwarf; galaxies: evolution; galaxies: formation; galaxies:
high-redshift; galaxies: starburst
ID STAR-FORMING GALAXIES; ACTIVE GALACTIC NUCLEI; DIGITAL SKY SURVEY;
HUBBLE-SPACE-TELESCOPE; GREATER-THAN 1; SIMILAR-TO 2; EXTRAGALACTIC
LEGACY SURVEY; HIGH-REDSHIFT GALAXIES; GREEN PEA GALAXIES; LOW-MASS
GALAXIES
AB We present near-infrared spectroscopy of a sample of 22 Extreme Emission Line Galaxies at redshifts 1.3 < z < 2.3, confirming that these are low-mass (M* = 108-109M(circle dot)) galaxies undergoing intense starburst episodes (M*/SFR similar to 10-100 Myr). The sample is selected by [O iii] or Ha emission line flux and equivalent width using near-infrared grism spectroscopy from the 3D-HST survey. High-resolution NIR spectroscopy is obtained with LBT/LUCI and VLT/X-SHOOTER. The [Oiii]/H line ratio is high (greater than or similar to 5) and [N ii]/Ha is always significantly below unity, which suggests a low gas-phase metallicity. We are able to determine gas-phase metallicities for seven of our objects using various strong-line methods, with values in the range 0.05-0.30 Z similar to and with a median of 0.15 Z similar to; for three of these objects we detect [O iii].4363, which allows for a direct constraint on the metallicity. The velocity dispersion, as measured from the nebular emission lines, is typically similar to 50 km s-1. Combined with the observed star-forming activity, the Jeans and Toomre stability criteria imply that the gas fraction must be large (fgas - 2/3), consistent with the difference between our dynamical and stellar mass estimates. The implied gas depletion timescale (several hundred Myr) is substantially longer than the inferred mass-weighted ages (similar to 50 Myr), which further supports the emerging picture that most stars in low-mass galaxies form in short, intense bursts of star formation.
C1 [Maseda, Michael V.; van der Wel, Arjen; Rix, Hans-Walter; da Cunha, Elisabete; Meidt, Sharon E.] Max Planck Inst Astron, D-69117 Heidelberg, Germany.
[Pacifici, Camilla] Yonsei Univ, Yonsei Univ Observ, Seoul 120749, South Korea.
[Momcheva, Ivelina; van Dokkum, Pieter; Nelson, Erica J.] Yale Univ, Dept Astron, New Haven, CT 06520 USA.
[Brammer, Gabriel B.; Ferguson, Henry C.; Koekemoer, Anton M.] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
[Franx, Marijn; Fumagalli, Mattia] Leiden Univ, Leiden Observ, Leiden, Netherlands.
[Bell, Eric F.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA.
[Foerster-Schreiber, Natascha M.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany.
[Koo, David C.] Univ Calif Santa Cruz, UCO Lick Observ, Santa Cruz, CA 95064 USA.
[Koo, David C.] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA.
[Lundgren, Britt F.] Univ Wisconsin, Dept Astron, Madison, WI 53706 USA.
[Marchesini, Danilo] Tufts Univ, Dept Phys & Astron, Medford, MA 02155 USA.
[Patel, Shannon G.] Carnegie Observ, Pasadena, CA 91101 USA.
[Skelton, Rosalind E.] S African Astron Observ, ZA-7935 Cape Town, South Africa.
[Straughn, Amber N.; Whitaker, Katherine E.] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA.
[Trump, Jonathan R.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA.
RP Maseda, MV (reprint author), Max Planck Inst Astron, Konigstuhl 17, D-69117 Heidelberg, Germany.
EM maseda@mpia.de
RI Skelton, Rosalind/S-1845-2016;
OI Skelton, Rosalind/0000-0001-7393-3336; Koekemoer,
Anton/0000-0002-6610-2048; da Cunha, Elisabete/0000-0001-9759-4797;
Bell, Eric/0000-0002-5564-9873; Brammer, Gabriel/0000-0003-2680-005X
FU KASI-Yonsei Joint Research Program for the Frontiers of Astronomy and
Space Science - Korea Astronomy and Space Science Institute; NSF
[AST-08-08133]
FX M. V. M. is a member of the International Max Planck Research School for
Astronomy and Cosmic Physics at the University of Heidelberg, IMPRS-HD,
Germany. C. P. acknowledges support by the KASI-Yonsei Joint Research
Program for the Frontiers of Astronomy and Space Science funded by the
Korea Astronomy and Space Science Institute. D. C. K. acknowledges
funding from NSF grant AST-08-08133. We would also like to thank R.
Amorin for productive discussions and C. Berlind and F. Rice for their
computational expertise.
NR 96
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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 AUG 10
PY 2014
VL 791
IS 1
AR 17
DI 10.1088/0004-637X/791/1/17
PG 17
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AM2CY
UT WOS:000339657700017
ER
PT J
AU McCullough, PR
Crouzet, N
Deming, D
Madhusudhan, N
AF McCullough, P. R.
Crouzet, N.
Deming, D.
Madhusudhan, N.
TI WATER VAPOR IN THE SPECTRUM OF THE EXTRASOLAR PLANET HD 189733b. I. THE
TRANSIT
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE planetary systems; planets and satellites: atmospheres; stars:
individual (HD 189733); techniques: spectroscopic
ID HUBBLE-SPACE-TELESCOPE; NICMOS TRANSMISSION SPECTROSCOPY; MU-M;
ATMOSPHERIC HAZE; GJ 1214B; STARS; ABSORPTION; TEMPERATURE; VARIABILITY;
EXOPLANETS
AB We report near-infrared spectroscopy of the gas giant planet HD 189733b in transit. We used the Hubble Space Telescope Wide Field Camera 3 (IIST WFC3) with its G141 grism covering 1.1 mu m to 1.7 mu m and spatially scanned the image across the detector at 2 '' s(-1). When smoothed to 75 nm bins, the local maxima of the transit depths in the 1.15 mu m and 1.4 mu m water vapor features are, respectively, 83 +/- 53 ppm and 200 +/- 47 ppm greater than the local minimum at 1.3 mu m. We compare the WFC3 spectrum with the composite transit spectrum of HD 189733b assembled by Pont et al., extending from 0.3 mu m to 24 mu m. Although the water vapor features in the WFC3 spectrum are compatible with the model of non-absorbing, Rayleigh-scattering dust in the planetary atmosphere, we also re-interpret the available data with a clear planetary atmosphere. In the latter interpretation, the slope of increasing transit depth with shorter wavelengths from the near infrared, through the visible, and into the ultraviolet is caused by unocculted star spots, with a smaller contribution of Rayleigh scattering by molecular hydrogen in the planet's atmosphere. At relevant pressures along the terminator, our model planetary atmosphere's temperature is similar to 700 K, which is below the condensation temperatures of sodium- and potassium-bearing molecules, causing the broad wings of the spectral lines of Na I and K I at 0.589 mu m and 0.769 mu m to be weak.
C1 [McCullough, P. R.; Crouzet, N.] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
[McCullough, P. R.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA.
[Crouzet, N.] Univ Toronto, Dunlap Inst Astron & Astrophys, Toronto, ON M5S 3H4, Canada.
[Deming, D.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Deming, D.] NASA, Astrobiol Inst, Virtual Planetary Lab, Washington, DC USA.
[Madhusudhan, N.] Yale Univ, Yale Ctr Astron & Astrophys, New Haven, CT 06511 USA.
[Madhusudhan, N.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England.
RP McCullough, PR (reprint author), Space Telescope Sci Inst, 3700 San Martin Dr, Baltimore, MD 21218 USA.
EM pmcc@stsci.edu
OI Crouzet, Nicolas/0000-0001-7866-8738
FU HST [GO-12881]; Origins of Solar Systems [NNX10AG30G]
FX This research used NASA's Astrophysics Data System Bibliographic
Services and the SIMBAD database, operated at CDS, Strasbourg, France,
and was funded in part by HST grant GO-12881 and Origins of Solar
Systems grant NNX10AG30G.
NR 65
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U1 1
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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 AUG 10
PY 2014
VL 791
IS 1
AR 55
DI 10.1088/0004-637X/791/1/55
PG 11
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AM2CY
UT WOS:000339657700055
ER
PT J
AU Sloan, GC
Lagadec, E
Zijlstra, AA
Kraemer, KE
Weis, AP
Matsuura, M
Volk, K
Peeters, E
Duley, WW
Cami, J
Bernard-Salas, J
Kemper, F
Sahai, R
AF Sloan, G. C.
Lagadec, E.
Zijlstra, A. A.
Kraemer, K. E.
Weis, A. P.
Matsuura, M.
Volk, K.
Peeters, E.
Duley, W. W.
Cami, J.
Bernard-Salas, J.
Kemper, F.
Sahai, R.
TI CARBON-RICH DUST PAST THE ASYMPTOTIC GIANT BRANCH: ALIPHATICS,
AROMATICS, AND FULLERENES IN THE MAGELLANIC CLOUDS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE circumstellar matter; infrared: stars
ID SPITZER-SPACE-TELESCOPE; INFRARED-EMISSION FEATURES; 21 MU-M;
GRAVITATIONAL LENSING EXPERIMENT.; SHORT-WAVELENGTH SPECTROMETER;
POINT-SOURCE CATALOG; OGLE-III CATALOG; POST-AGB STARS;
PLANETARY-NEBULAE; PROTOPLANETARY NEBULAE
AB Infrared spectra of carbon-rich objects that have evolved off the asymptotic giant branch reveal a range of dust properties, including fullerenes, polycyclic aromatic hydrocarbons (PAHs), aliphatic hydrocarbons, and several unidentified features, including the 21 mu m emission feature. To test for the presence of fullerenes, we used the position and width of the feature at 18.7-18.9 mu m and examined other features at 17.4 and 6-9 mu m. This method adds three new fullerene sources to the known sample, but it also calls into question three previous identifications. We confirm that the strong 11 mu m features seen in some sources arise primarily from SiC, which may exist as a coating around carbonaceous cores and result from photo-processing. Spectra showing the 21 mu m feature usually show the newly defined Class D PAH profile at 7-9 mu m. These spectra exhibit unusual PAH profiles at 11-14 mu m, with weak contributions at 12.7 mu m, which we define as Class D1, or show features shifted to similar to 11.4, 12.4, and 13.2 mu m, which we define as Class D2. Alkyne hydrocarbons match the 15.8 mu m feature associated with 21 mu m emission. Sources showing fullerene emission but no PAHs have blue colors in the optical, suggesting a clear line of sight to the central source. Spectra with 21 mu m features and Class D2 PAH emission also show photometric evidence for a relatively clear line of sight to the central source. The multiple associations of the 21 mu m feature with aliphatic hydrocarbons suggest that the carrier is related to this material in some way.
C1 [Sloan, G. C.; Lagadec, E.] Cornell Univ, Ctr Radiophys & Space Res, Ithaca, NY 14853 USA.
[Zijlstra, A. A.] Univ Manchester, Jodrell Bank Ctr Astrophys, Manchester M13 9PL, Lancs, England.
[Kraemer, K. E.] Boston Coll, Inst Sci Res, Chestnut Hill, MA 02467 USA.
[Weis, A. P.] Columbia Univ, Dept Astron & Astrophys, New York, NY 10027 USA.
[Weis, A. P.] Cornell Univ, Dept Astron, Ithaca, NY 14853 USA.
[Matsuura, M.] UCL, Dept Phys & Astron, Astrophys Grp, London WC1E 6BT, England.
[Volk, K.] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
[Peeters, E.; Cami, J.] Univ Western Ontario, Dept Phys & Astron, London, ON N6A 3K7, Canada.
[Peeters, E.; Cami, J.] SETI Inst, Mountain View, CA 94043 USA.
[Duley, W. W.] Univ Waterloo, Dept Phys & Astron, Waterloo, ON N2L 3G1, Canada.
[Bernard-Salas, J.] Open Univ, Dept Phys Sci, Milton Keynes MK7 6AA, Bucks, England.
[Kemper, F.] Acad Sinica, Inst Astron & Astrophys, NTU AS, Taipei 10617, Taiwan.
[Sahai, R.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Sloan, GC (reprint author), Cornell Univ, Ctr Radiophys & Space Res, Ithaca, NY 14853 USA.
EM sloan@isc.astro.cornell.edu
RI Kemper, Francisca/D-8688-2011;
OI Kemper, Francisca/0000-0003-2743-8240; Kraemer,
Kathleen/0000-0002-2626-7155
FU NASA [1257184]; California Institute of Technology under NASA [1407];
National Science Council of Taiwan [NSC100-2112-M-001-023-MY3]
FX We thank the referee, A. P. Jones, for a thorough report that led to
substantial improvements in this paper. We are grateful to P. R. Wood
for providing the spectrum of LIN 49. G.C.S. was supported by NASA
through Contract Number 1257184 issued by the Jet Propulsion Laboratory,
California Institute of Technology under NASA contract 1407. F.K.
received support from the National Science Council of Taiwan, grant
NSC100-2112-M-001-023-MY3. This research relied on the following
resources: NASA's Astrophysics Data System, the Infrared Science Archive
at the Infrared Processing and Analysis Center, operated by JPL, and the
SIMBAD and VizieR databases, operated at the Centre de Donnees
astronomiques de Strasbourg.
NR 98
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U1 1
U2 8
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 AUG 10
PY 2014
VL 791
IS 1
AR 28
DI 10.1088/0004-637X/791/1/28
PG 30
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AM2CY
UT WOS:000339657700028
ER
PT J
AU Taquet, V
Charnley, SB
Sipila, O
AF Taquet, Vianney
Charnley, Steven B.
Sipila, Olli
TI MULTILAYER FORMATION AND EVAPORATION OF DEUTERATED ICES IN PRESTELLAR
AND PROTOSTELLAR CORES
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE astrochemistry; ISM: abundances; ISM: molecules; stars: formation
ID DENSE INTERSTELLAR CLOUDS; SOLAR-TYPE PROTOSTARS; WATER DEUTERIUM
FRACTIONATION; COMPLEX ORGANIC-MOLECULES; GRAIN SURFACE-CHEMISTRY;
STAR-FORMING REGIONS; LOW-MASS PROTOSTARS; O1 HALE-BOPP; IRAS
16293-2422; INFALL MOTIONS
AB Extremely large deuteration of several molecules has been observed toward prestellar cores and low-mass protostars for a decade. New observations performed toward low-mass protostars suggest that water presents a lower deuteration in the warm inner gas than in the cold external envelope. We coupled a gas-grain astrochemical model with a one-dimensional model of a collapsing core to properly follow the formation and the deuteration of interstellar ices as well as their subsequent evaporation in the low-mass protostellar envelopes with the aim of interpreting the spatial and temporal evolutions of their deuteration. The astrochemical model follows the formation and the evaporation of ices with a multilayer approach and also includes a state-of-the-art deuterated chemical network by taking the spin states of H-2 and light ions into account. Because of their slow formation, interstellar ices are chemically heterogeneous and show an increase of their deuterium fractionation toward the surface. The differentiation of the deuteration in ices induces an evolution of the deuteration within protostellar envelopes. The warm inner region is poorly deuterated because it includes the whole molecular content of ices, while the deuteration predicted in the cold external envelope scales with the highly deuterated surface of ices. We are able to reproduce the observed evolution of water deuteration within protostellar envelopes, but we are still unable to predict the super-high deuteration observed for formaldehyde and methanol. Finally, the extension of this study to the deuteration of complex organics, important for the prebiotic chemistry, shows good agreement with the observations, suggesting that we can use the deuteration to retrace their mechanisms and their moments of formation.
C1 [Taquet, Vianney; Charnley, Steven B.] NASA, Goddard Space Flight Ctr, Astrochem Lab, Greenbelt, MD 20770 USA.
[Taquet, Vianney; Charnley, Steven B.] NASA, Goddard Space Flight Ctr, Goddard Ctr Astrobiol, Greenbelt, MD 20770 USA.
[Sipila, Olli] Univ Helsinki, Dept Phys, FI-00014 Helsinki, Finland.
RP Taquet, V (reprint author), NASA, Goddard Space Flight Ctr, Astrochem Lab, Mailstop 691,8800 Greenbelt Rd, Greenbelt, MD 20770 USA.
FU NASA's Origins of Solar Systems and Exobiology Programs; NASA
postdoctoral program; Academy of Finland [250741]
FX The kinetic data we used have been downloaded from the online database
KIDA (Wakelam et al.2012; http://kida.obs.ubordeaux1.fr). This work was
supported by NASA's Origins of Solar Systems and Exobiology Programs.
V.T. acknowledges support from the NASA postdoctoral program. O.S.
acknowledges support from the Academy of Finland grant 250741.
NR 140
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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 AUG 10
PY 2014
VL 791
IS 1
AR 1
DI 10.1088/0004-637X/791/1/1
PG 20
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AM2CY
UT WOS:000339657700001
ER
PT J
AU Zaccheo, TS
Pernini, T
Snell, HE
Browell, EV
AF Zaccheo, T. Scott
Pernini, Timothy
Snell, Hilary E.
Browell, Edward V.
TI Impact of atmospheric state uncertainties on retrieved XCO2 columns from
laser differential absorption spectroscopy measurements
SO JOURNAL OF APPLIED REMOTE SENSING
LA English
DT Article
DE laser absorption spectroscopy; lidar; CO2 retrievals; ASCENDS
ID CONSTRAINED MULTISPECTRUM ANALYSIS; SPEED DEPENDENCE; CO2; LIDAR;
INTENSITIES; CM(-1)
AB This work assesses the impact of uncertainties in atmospheric state knowledge on retrievals of carbon dioxide column amounts (XCO2) from laser differential absorption spectroscopy (LAS) measurements. LAS estimates of XCO2 columns are normally derived not only from differential absorption observations but also from measured or prior knowledge of atmospheric state that includes temperature, moisture, and pressure along the viewing path. In the case of global space-based monitoring systems, it is often difficult if not impossible to provide collocated in situ measurements of atmospheric state for all observations, so retrievals often rely on collocated remote-sensed data or values derived from numerical weather prediction (NWP) models to describe the atmospheric state. A radiative transfer-based simulation framework, combined with representative global upper-air observations and matched NWP profiles, was used to assess the impact of model differences on estimates of column CO2 and O-2 concentrations. These analyses focus on characterizing these errors for LAS measurements of CO2 in the 1.57-mu m region and of O-2 in the 1.27-mu m region. The results provide a set of signal-to-noise metrics that characterize the errors in retrieved values associated with uncertainties in atmospheric state and provide a method for selecting optimal differential absorption line pairs to minimize the impact of these noise terms. (C) The Authors. Published by SPIE under a Creative Commons Attribution 3.0 Unported License.
C1 [Zaccheo, T. Scott; Pernini, Timothy; Snell, Hilary E.] Atmospher & Environm Res Inc, Lexington, MA 02421 USA.
[Browell, Edward V.] NASA, STARSS Affiliate 2, Langley Res Ctr, Yorktown, VA 23692 USA.
RP Zaccheo, TS (reprint author), Atmospher & Environm Res Inc, 131 Hartwell Ave, Lexington, MA 02421 USA.
EM szaccheo@aer.com
FU NASA Langley Research Center, ASCENDS CarbonHawk Experiment Simulator
(ACES) project - NASA Earth Science Technology Office, Instrument
Incubator Program [NNL11AD10T]; Atmospheric and Environmental Research,
Inc. management
FX This work has been supported in part by a contract to AER from NASA
Langley Research Center as part of the ASCENDS CarbonHawk Experiment
Simulator (ACES) project funded under the NASA Earth Science Technology
Office, Instrument Incubator Program (order # NNL11AD10T). The authors
would like to thank a number of their colleagues at the NASA Langley
Research Center: Narasimha Prasad for his hard work and dedication that
enabled the ACES program to come to fruition, and F. Wallace Harrison,
Syed Ismail, and Michael D. Obland for their continued support and
insights that has allowed this work to move forward. Additionally, we
would like to thank the anonymous JARS reviewer, whose in depth feedback
have significantly strengthened the readability and content of this
work. Finally, we would like to acknowledge Atmospheric and
Environmental Research, Inc. management for their support of this effort
over a number of years.
NR 18
TC 2
Z9 2
U1 2
U2 10
PU SPIE-SOC PHOTO-OPTICAL INSTRUMENTATION ENGINEERS
PI BELLINGHAM
PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98225 USA
SN 1931-3195
J9 J APPL REMOTE SENS
JI J. Appl. Remote Sens.
PD AUG 8
PY 2014
VL 8
AR 083575
DI 10.1117/1.JRS.8.083575
PG 16
WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic
Technology
SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science &
Photographic Technology
GA AP8UE
UT WOS:000342353900001
ER
PT J
AU Mikellides, IG
Hofer, RR
Katz, I
Goebel, DM
AF Mikellides, Ioannis G.
Hofer, Richard R.
Katz, Ira
Goebel, Dan M.
TI Magnetic shielding of Hall thrusters at high discharge voltages
SO JOURNAL OF APPLIED PHYSICS
LA English
DT Article
AB A series of numerical simulations and experiments have been performed to assess the effectiveness of magnetic shielding in a Hall thruster operating in the discharge voltage range of 300-700V (I-sp approximate to 2000-2700 s) at 6 kW, and 800V (I-sp approximate to 3000) at 9 kW. At 6 kW, the magnetic field topology with which highly effective magnetic shielding was previously demonstrated at 300V has been retained for all other discharge voltages; only the magnitude of the field has been changed to achieve optimum thruster performance. It is found that magnetic shielding remains highly effective for all discharge voltages studied. This is because the channel is long enough to allow hot electrons near the channel exit to cool significantly upon reaching the anode. Thus, despite the rise of the maximum electron temperature in the channel with discharge voltage, the electrons along the grazing lines of force remain cold enough to eliminate or reduce significantly parallel gradients of the plasma potential near the walls. Computed maximum erosion rates in the range of 300-700V are found not to exceed 10(-2) mm/kh. Such rates are similar to 3 orders of magnitude less than those observed in the unshielded version of the same thruster at 300V. At 9 kW and 800 V, saturation of the magnetic circuit did not allow for precisely the same magnetic shielding topology as that employed during the 6-kW operation since this thruster was not designed to operate at this condition. Consequently, the maximum erosion rate at the inner wall is found to be similar to 1 order of magnitude higher (similar to 10(-1) mm/kh) than that at 6 kW. At the outer wall, the ion energy is found to be below the sputtering yield threshold so no measurable erosion is expected. (C) 2014 AIP Publishing LLC.
C1 [Mikellides, Ioannis G.; Hofer, Richard R.; Katz, Ira; Goebel, Dan M.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Mikellides, IG (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM Ioannis.G.Mikellides@jpl.nasa.gov
FU National Aeronautics and Space Administration
FX The research described in this paper was carried out by the Jet
Propulsion Laboratory, California Institute of Technology, under a
contract with the National Aeronautics and Space Administration and
funded through the internal Research and Technology Development program.
The authors wish to acknowledge Dr. Benjamin A. Jorns for providing the
applied magnetic field measurements in the 9MS800 configuration of the
H6 thruster.
NR 22
TC 5
Z9 5
U1 0
U2 15
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
EI 1089-7550
J9 J APPL PHYS
JI J. Appl. Phys.
PD AUG 7
PY 2014
VL 116
IS 5
AR 053302
DI 10.1063/1.4892160
PG 11
WC Physics, Applied
SC Physics
GA AO2TM
UT WOS:000341178900008
ER
PT J
AU Kobayashi, DR
Farman, R
Polovina, JJ
Parker, DM
Rice, M
Balazs, GH
AF Kobayashi, Donald R.
Farman, Richard
Polovina, Jeffrey J.
Parker, Denise M.
Rice, Marc
Balazs, George H.
TI "Going with the Flow'' or Not: Evidence of Positive Rheotaxis in Oceanic
Juvenile Loggerhead Turtles (Caretta caretta) in the South Pacific Ocean
Using Satellite Tags and Ocean Circulation Data
SO PLOS ONE
LA English
DT Article
ID CENTRAL NORTH PACIFIC; OLIVACEA SEA-TURTLES; ORIENTATION; MOVEMENT;
BEHAVIOR; CURRENTS; HABITAT; DESIGN; MODEL
AB The movement of juvenile loggerhead turtles (n = 42) out-fitted with satellite tags and released in oceanic waters off New Caledonia was examined and compared with ocean circulation data. Merging of the daily turtle movement data with drifter buoy movements, OSCAR (Ocean Surface Current Analyses - Real time) circulation data, and three different vertical strata (05 m, 0-40 m, 0-100 m) of HYCOM (HYbrid Coordinate Ocean Model) circulation data indicated the turtles were swimming against the prevailing current in a statistically significant pattern. This was not an artifact of prevailing directions of current and swimming, nor was it an artifact of frictional slippage. Generalized additive modeling was used to decompose the pattern of swimming into spatial and temporal components. The findings are indicative of a positive rheotaxis whereby an organism is able to detect the current flow and orient itself to swim into the current flow direction or otherwise slow down its movement. Potential mechanisms for the means and adaptive significance of rheotaxis in oceanic juvenile loggerhead turtles are discussed.
C1 [Kobayashi, Donald R.; Polovina, Jeffrey J.; Balazs, George H.] NOAA, Pacific Islands Fisheries Sci Ctr, Natl Marine Fisheries Serv, Honolulu, HI 96813 USA.
[Farman, Richard] Aquarium Lagons, Noumea, New Caledonia.
[Parker, Denise M.] Univ Hawaii, Joint Inst Marine & Atmospher Res, Newport, OR USA.
[Rice, Marc] Hawaii Preparatory Acad, Kamuela, HI USA.
RP Kobayashi, DR (reprint author), NOAA, Pacific Islands Fisheries Sci Ctr, Natl Marine Fisheries Serv, Honolulu, HI 96813 USA.
EM Donald.Kobayashi@noaa.gov
FU United States government to National Oceanic and Atmospheric
Administration
FX The funders were base funding and add-on funding from the United States
government to National Oceanic and Atmospheric Administration and had no
role in study design, data collection and analysis, decision to publish,
or preparation of the manuscript.
NR 45
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Z9 11
U1 0
U2 17
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 AUG 6
PY 2014
VL 9
IS 8
AR e103701
DI 10.1371/journal.pone.0103701
PG 14
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA AM6SM
UT WOS:000339995100025
PM 25098694
ER
PT J
AU Forouhar, S
Borgentun, C
Frez, C
Briggs, RM
Bagheri, M
Canedy, CL
Kim, CS
Kim, M
Bewley, WW
Merritt, CD
Abell, J
Vurgaftman, I
Meyer, JR
AF Forouhar, S.
Borgentun, C.
Frez, C.
Briggs, R. M.
Bagheri, M.
Canedy, C. L.
Kim, C. S.
Kim, M.
Bewley, W. W.
Merritt, C. D.
Abell, J.
Vurgaftman, I.
Meyer, J. R.
TI Reliable mid-infrared laterally-coupled distributed-feedback interband
cascade lasers
SO APPLIED PHYSICS LETTERS
LA English
DT Article
ID HIGH-POWER
AB We report on the performance and reliability of laterally-coupled distributed-feedback (DFB) interband cascade lasers designed to operate at 3.6 mu m wavelength. A two-step ridge etch process ensures single-transverse-mode operation with minimal lateral current spreading, and a secondorder Bragg grating etched alongside the ridge waveguide imposes single-mode DFB operation. Life tests performed on four randomly selected lasers, continuously operating at 40 degrees C with output power >10 mW, showed no measurable degradation after each laser was operated continuously for more than 1500 h. (C) 2014 AIP Publishing LLC.
C1 [Forouhar, S.; Borgentun, C.; Frez, C.; Briggs, R. M.; Bagheri, M.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Canedy, C. L.; Kim, C. S.; Bewley, W. W.; Merritt, C. D.; Abell, J.; Vurgaftman, I.; Meyer, J. R.] Naval Res Lab, Washington, DC 20375 USA.
[Kim, M.] Sotera Def Solut Inc, Columbia, MD 21046 USA.
RP Forouhar, S (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM siamak.forouhar@jpl.nasa.gov
NR 17
TC 17
Z9 17
U1 0
U2 13
PU AMER INST PHYSICS
PI MELVILLE
PA 1305 WALT WHITMAN RD, STE 300, MELVILLE, NY 11747-4501 USA
SN 0003-6951
EI 1077-3118
J9 APPL PHYS LETT
JI Appl. Phys. Lett.
PD AUG 4
PY 2014
VL 105
IS 5
AR 051110
DI 10.1063/1.4892655
PG 4
WC Physics, Applied
SC Physics
GA AO2LE
UT WOS:000341153000010
ER
PT J
AU de Jeu, RAM
Holmes, TRH
Parinussa, RM
Owe, M
AF de Jeu, Richard A. M.
Holmes, Thomas R. H.
Parinussa, Robert M.
Owe, Manfred
TI A spatially coherent global soil moisture product with improved temporal
resolution
SO JOURNAL OF HYDROLOGY
LA English
DT Article
DE Soil moisture; Dielectric constant; Passive microwave radiometry; Remote
sensing
ID VEGETATION OPTICAL DEPTH; PASSIVE MICROWAVE OBSERVATIONS; POLARIZATION
DIFFERENCE INDEX; AMSR-E; SATELLITE-OBSERVATIONS; RETRIEVAL; MODEL;
VALIDATION; CLIMATE; FIELDS
AB Global soil moisture products that are completely independent of any type of ancillary data and solely rely on satellite observations are presented. Additionally, we further develop an existing downscaling technique that enhances the spatial resolution of such products to approximately 11 km. These products are based on internal modules of the Land Parameter Retrieval Model (LPRM), an algorithm that uses the radiative transfer equation to link soil moisture, vegetation optical depth and land surface temperature to observed brightness temperatures.
The soil moisture product that is independent of any type of ancillary data uses the internally calculated dielectric constant as a soil moisture proxy. This data product is not influenced by errors associated with coarse-scale global soil property maps or by any other type of forcing (e.g. re-analysis) data and is therefore solely based on satellite microwave observations. The second step builds upon recent developments to increase the spatial resolution of the LPRM retrievals using a smoothing filter downscaling method. With this method we can attain a spatial resolution that can be more useful at the scale of local and regional hydrological studies as well. The steps presented in this paper were applied to observations from the Advanced Microwave Scanning Radiometer-Earth Observing System (AMSR-E). The newly derived data sets were validated using ground-based observations from the International Soil Moisture Network (ISMN).
The internally calculated dielectric constant product results in significantly more days with valid retrievals than the original soil moisture data products, in particular over arid regions. The dielectric constant product resulted in similar correlations with in situ data as the original soil moisture data product. Together, these findings demonstrate the usefulness of this new dielectric constant product for the hydrological modeling community and climate studies. A case study on the Australian Fitzroy catchment demonstrated that the downscaled data product has a more detailed spatial description of soil moisture, especially during wet and dry conditions with more pronounced dry and wet regions within the catchment. The increased resolution data products could therefore improve runoff predictions and this study demonstrated the potential added value of a transitioning from a spatial resolution of 56 km toward a higher resolution of 11 km. The hydrological implications of these newly developed data records are not only linked to AMSR-E satellite data, but also to the next generation Soil Moisture Active and Passive (SMAP) mission where a 9 km spatial resolution is the target resolution for satellite soil moisture products. The new data products will not replace the current LPRM products, but will be added to the existing array of data products and will become publicly available through our data portals. (C) 2014 Elsevier B.V. All rights reserved.
C1 [de Jeu, Richard A. M.; Parinussa, Robert M.] Vrije Univ Amsterdam, Dept Earth Sci Earth & Climate Cluster, NL-1081 HV Amsterdam, Netherlands.
[Holmes, Thomas R. H.] ARS, USDA, Hydrol & Remote Sensing Lab, Beltsville, MD 20705 USA.
[Owe, Manfred] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20770 USA.
RP de Jeu, RAM (reprint author), Vrije Univ Amsterdam, Dept Earth Sci Earth & Climate Cluster, De Boelelaan 1085, NL-1081 HV Amsterdam, Netherlands.
EM r.a.m.de.jeu@vu.nl
RI Holmes, Thomas/F-4512-2010
OI Holmes, Thomas/0000-0002-4651-0079
FU European Space Agency Climate Change Initiative for soil moisture
[4000104814/11/I-NB]; European Commission [282672]
FX This work has been undertaken as part of the European Space Agency
Climate Change Initiative for soil moisture
(http://www.esa-soilmoisture-cci.org/), Contract No. 4000104814/11/I-NB)
Additionally, this work was funded by the European Commission's 7th
Framework Project, under Grant Agreement Number 282672, EMBRACE Project.
The authors would like to thank the International Soil Moisture Network
for making the verification data available. Finally, the authors would
like to thank Dr. I. van Meerveld for her valuable contribution to this
manuscript.
NR 70
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U1 2
U2 35
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0022-1694
EI 1879-2707
J9 J HYDROL
JI J. Hydrol.
PD AUG 4
PY 2014
VL 516
SI SI
BP 284
EP 296
DI 10.1016/j.jhydrol.2014.02.015
PG 13
WC Engineering, Civil; Geosciences, Multidisciplinary; Water Resources
SC Engineering; Geology; Water Resources
GA AL3NT
UT WOS:000339036100026
ER
PT J
AU Stephens, DB
Vold, H
AF Stephens, David B.
Vold, Havard
TI Order tracking signal processing for open rotor acoustics
SO JOURNAL OF SOUND AND VIBRATION
LA English
DT Article
ID SHAFT-SPEED INFORMATION; KALMAN; EXPLORATION; FILTER
AB Counter-rotating open rotor acoustic measurements were processed using a two-shaft Vold-Kalman order tracking filter, providing new insight into the complicated noise generation mechanisms of this type of system. The multi-shaft formulation of the Vold-Kalman filter can determine a time-accurate output of shaft order tones associated with each rotor, even as the rotation rate of the two rotors varies. This is a major improvement over the usual short time Fourier transform method for many applications. It was found that the contribution from each rotor to the individual tones varies strongly as a function of shaft order and operating condition. The order tracking filter is also demonstrated as a robust tool for separating the tonal and broadband components of a signal for which the usual shaft phase averaging methods fail. Published by Elsevier Ltd.
C1 [Stephens, David B.] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA.
[Vold, Havard] ATA Engn Inc, San Diego, CA 92103 USA.
RP Stephens, DB (reprint author), NASA, Glenn Res Ctr, Cleveland, OH 44135 USA.
EM david.stephens@nasa.gov; hvold@ata-e.com
FU NASA Fixed Wing project; ATA Engineering, Inc. [SAA3-1239]
FX This paper was funded by the NASA Fixed Wing project with Dr. Ruben Del
Rosario as the project manager. The authors would also like to thank ATA
Engineering, Inc., for their support and usage of proprietary software.
The work was performed under the Space Act Agreement: SAA3-1239, ATA
Engineering, Inc., "Joint Publication On Order Tracking Methods For
Quantifying Noise From Open Rotors." The open rotor wind tunnel test was
performed as a collaboration between the NASA Environmentally
Responsible Aviation project and GE Aviation.
NR 25
TC 2
Z9 2
U1 0
U2 4
PU ACADEMIC PRESS LTD- ELSEVIER SCIENCE LTD
PI LONDON
PA 24-28 OVAL RD, LONDON NW1 7DX, ENGLAND
SN 0022-460X
EI 1095-8568
J9 J SOUND VIB
JI J. Sound Vibr.
PD AUG 4
PY 2014
VL 333
IS 16
BP 3818
EP 3830
DI 10.1016/j.jsv.2014.04.005
PG 13
WC Acoustics; Engineering, Mechanical; Mechanics
SC Acoustics; Engineering; Mechanics
GA AI4FY
UT WOS:000336822300016
ER
PT J
AU Laurini, KC
Gerstenmaier, WH
AF Laurini, Kathleen C.
Gerstenmaier, William H.
TI The Global Exploration Roadmap and its significance for NASA
SO SPACE POLICY
LA English
DT Article
DE Global Exploration Roadmap; NASA; International cooperation
AB The Global Exploration Roadmap reflects the collaborative effort of twelve space agencies to define a long-term human space exploration strategy which provides substantial benefits for improving the quality of life on Earth and is implementable and sustainable. Such a strategy is a necessary precondition to the government investments required to enable the challenging and rewarding missions that extend human presence into the solar system. The article introduces the international strategy and elaborates on NASA's leadership role in shaping that strategy. The publication of the roadmap, a reflection of the space landscape and multilateral agency-level dialog over the last four years, allows NASA to demonstrate its commitment to leading a long-term space exploration endeavor that delivers benefits, maintains strategic human spaceflight capabilities and expands human presence in space, with human missions to the surface of Mars as a driving goal. The road mapping process has clearly demonstrated the complementary interests of the participants and the potential benefits that can be gained through cooperation among nations to achieve a common goal. The present US human spaceflight policy is examined and it is shown that the establishment of a sustainable global space exploration strategy is fully consistent with that policy. Published by Elsevier Ltd.
C1 [Laurini, Kathleen C.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA.
[Gerstenmaier, William H.] NASA, Washington, DC 20546 USA.
RP Laurini, KC (reprint author), NASA, Lyndon B Johnson Space Ctr, 2101 NASA Pkwy, Houston, TX 77058 USA.
EM Kathy.laurini-1@nasa.gov
NR 21
TC 0
Z9 0
U1 3
U2 7
PU ELSEVIER SCI LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND
SN 0265-9646
EI 1879-338X
J9 SPACE POLICY
JI Space Policy
PD AUG
PY 2014
VL 30
IS 3
SI SI
BP 149
EP 155
DI 10.1016/j.spacepol.2014.08.004
PN B
PG 7
WC International Relations; Social Sciences, Interdisciplinary
SC International Relations; Social Sciences - Other Topics
GA AY5HL
UT WOS:000347603300004
ER
PT J
AU Neal, CR
Schmidt, GK
Ehrenfreund, P
Carpenter, JD
AF Neal, C. R.
Schmidt, G. K.
Ehrenfreund, P.
Carpenter, J. D.
TI Developing the global exploration roadmap: An example using the humans
to the lunar surface theme
SO SPACE POLICY
LA English
DT Article
DE Space exploration; Lunar exploration; Global exploration roadmap; Test
bed
ID SPACE EXPLORATION; EPITHERMAL NEUTRONS; WATER ICE; MOON; CRATERS;
PROJECT; SCIENCE; POLES; RADAR
AB The development of the Global Exploration Roadmap (GER) by 12 space agencies participating in the International Space Exploration Coordination Group broadly outlines a pathway to send humans beyond low Earth orbit for the first time since Apollo. Three themes have emerged: Exploration of a Near-Earth Asteroid, Extended Duration Crew Missions, and Humans to the Lunar Surface. The lack of detail within each of these themes could mean that realizing the goals of the GER would be significantly delayed. The purpose of this paper is to demonstrate that many of the details needed to fully define and evaluate these themes in terms of scientific rationale, economic viability, and technical feasibility already exist and need to be mapped to the GER. Here, we use the Humans to the Lunar Surface theme as an example to illustrate how this process could work. By mapping documents from a variety of international stake-holders, this process can be used to cement buy-in from the current partners and attract new ones to this effort. (C) 2014 Published by Elsevier Ltd.
C1 [Neal, C. R.] Univ Notre Dame, Dept Civil & Environm Engn & Earth Sci, Notre Dame, IN 46556 USA.
[Schmidt, G. K.] NASA, Ames Res Ctr, SSERVI, Moffett Field, CA 94035 USA.
[Ehrenfreund, P.] George Washington Univ, Inst Space Policy, Washington, DC 20052 USA.
[Carpenter, J. D.] ESA ESTEC, NL-2401 AZ Noordwijk, Netherlands.
RP Neal, CR (reprint author), Univ Notre Dame, Dept Civil & Environm Engn & Earth Sci, Notre Dame, IN 46556 USA.
EM cneal@nd.edu; gregory.k.schmidt@nasa.gov; pehren@gwu.edu;
james.carpenter@esa.int
NR 46
TC 1
Z9 1
U1 1
U2 1
PU ELSEVIER SCI LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND
SN 0265-9646
EI 1879-338X
J9 SPACE POLICY
JI Space Policy
PD AUG
PY 2014
VL 30
IS 3
SI SI
BP 156
EP 162
DI 10.1016/j.spacepol.2014.08.007
PN B
PG 7
WC International Relations; Social Sciences, Interdisciplinary
SC International Relations; Social Sciences - Other Topics
GA AY5HL
UT WOS:000347603300005
ER
PT J
AU Ehrenfreund, P
McKay, CP
AF Ehrenfreund, P.
McKay, C. P.
CA COSPAR Panel Exploration PEX
TI Activities of the COSPAR Panel on Exploration supporting the Global
Exploration Roadmap
SO SPACE POLICY
LA English
DT Editorial Material
DE Space exploration; International cooperation; Solar system
AB The Global Exploration Roadmap (GER) is driven by several goals and objectives that include space science, the search for life as well as preparatory science activities to enable human space exploration. The Committee on Space Research (COSPAR), through its Commissions and Panels provides an international forum that supports and promotes space exploration worldwide. COSPAR's Panel on Exploration (PEX) investigates a stepwise approach of preparatory research on Earth and in Low Earth Orbit (LEO) to facilitate a future global space exploration program. We summarize recent activities and workshops of PEX in support of the GER. (C) 2014 Elsevier Ltd. All rights reserved.
C1 [Ehrenfreund, P.] George Washington Univ, Elliott Sch Int Affairs, Inst Space Policy, Washington, DC 20052 USA.
[McKay, C. P.] NASA, Ames Res Ctr, Mountain View, CA 94035 USA.
RP Ehrenfreund, P (reprint author), George Washington Univ, Elliott Sch Int Affairs, Inst Space Policy, 1957 E St,Suite 403, Washington, DC 20052 USA.
EM pehren@gwu.edu
NR 10
TC 0
Z9 0
U1 0
U2 1
PU ELSEVIER SCI LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND
SN 0265-9646
EI 1879-338X
J9 SPACE POLICY
JI Space Policy
PD AUG
PY 2014
VL 30
IS 3
SI SI
BP 170
EP 173
DI 10.1016/j.spacepol.2014.07.006
PN B
PG 4
WC International Relations; Social Sciences, Interdisciplinary
SC International Relations; Social Sciences - Other Topics
GA AY5HL
UT WOS:000347603300007
ER
PT J
AU Brown, ME
Carroll, ML
Escobar, VM
AF Brown, Molly E.
Carroll, Mark L.
Escobar, Vanessa M.
TI User needs and assessing the impact of low latency NASA Earth
observation data availability on societal benefit
SO SPACE POLICY
LA English
DT Article
DE NASA; Latency; Earth observation; Applications; Operational; Satellite
data
AB Since the advent of NASA's Earth Observing System, knowledge of the practical benefits of Earth science data has grown considerably. The community using NASA Earth science observations in applications has grown significantly, with increasing sophistication to serve national interests. Data latency, or how quickly communities receive science observations after acquisition, can have a direct impact on the applications and usability of the information. This study was conducted to determine how users are incorporating NASA data into applications and operational processes to benefit society beyond scientific research, as well as to determine the need for data latency of less than 12 h. The results of the analysis clearly show the significant benefit to society of serving the needs of the agricultural, emergency response, environmental monitoring and weather communities who use rapidly delivered, accurate Earth science data. The study also showed the potential of expanding the communities who use low latency NASA science data products to provide new ways of transforming data into information. These benefits can be achieved with a clear and consistent NASA policy on product latency. Published by Elsevier Ltd.
C1 [Brown, Molly E.] NASA, Goddard Space Flight Ctr, Biospher Sci Lab, Greenbelt, MD 20771 USA.
[Carroll, Mark L.; Escobar, Vanessa M.] NASA, Goddard Space Flight Ctr, Sigma Space Corp, Greenbelt, MD 20771 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 8
TC 0
Z9 0
U1 0
U2 2
PU ELSEVIER SCI LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND
SN 0265-9646
EI 1879-338X
J9 SPACE POLICY
JI Space Policy
PD AUG
PY 2014
VL 30
IS 3
BP 135
EP 137
DI 10.1016/j.spacepol.2014.05.002
PN A
PG 3
WC International Relations; Social Sciences, Interdisciplinary
SC International Relations; Social Sciences - Other Topics
GA AY5HK
UT WOS:000347603200003
ER
PT J
AU Burlaga, LF
Ness, NF
Richardson, JD
AF Burlaga, L. F.
Ness, N. F.
Richardson, J. D.
TI Heliosheath magnetic field and plasma observed by Voyager 2 during 2011
SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS
LA English
DT Article
ID TERMINATION SHOCK; SOLAR-WIND; STRENGTH FLUCTUATIONS; AU; INTENSITIES;
CYCLE
AB We discuss magnetic field and plasma observations from Voyager 2 (V2) during 2011, when V2 was beginning to see the effects of increasing solar activity following the solar minimum in 2009. The magnetic field strength (B) profile showed large amplitude fluctuations that can be resolved into a linear increase of B with time and a sinusoidal variation of the period of 86.2 +/- 0.8 days. Voyager 2 was in a unipolar region in which the magnetic polarity was directed away from the Sun along the Parker spiral 96% of the time, indicating that V2 was poleward of the heliospheric current sheet throughout most of 2011. The distribution of B was lognormal, but a Gaussian distribution was observed when the linear variation of B was subtracted from the data. The distribution of daily increments of B was a q-Gaussian distribution with q = 1.1 +/- 0.1, which is less intermittent than normally observed in the heliosheath. However, the distribution of hourly increments of B was a q-Gaussian distribution with q = 1.5 +/- 0.03. The density, temperature, and velocity increased linearly from the beginning of 2011 to approximately day 254. The magnetic and thermal pressure tended to increase throughout the year, but the magnetic pressure dominated most of the time. The counting rate of > 70 MeV/nucleon particles increased rapidly during the first 250 days, but it leveled out during the rest of the year when B was stronger. The empirical CR-B relationship describes this behavior.
C1 [Burlaga, L. F.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Ness, N. F.] Catholic Univ Amer, Inst Astrophys & Computat Sci, Washington, DC 20064 USA.
[Richardson, J. D.] MIT, Kalvi Ctr Astrophys & Space Res, Cambridge, MA 02139 USA.
RP Burlaga, LF (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
EM lburlagahsp@verizon.net
FU NASA [NNG14PN24P]; NASA from the JPL [959203]; [NNX12A63G]
FX The data in this paper are from the magnetic field experiment on Voyager
2. N.F. Ness was partially supported by grant NNX12A63G to Catholic
University of America. L. F. Burlaga was supported by NASA grant
NNG14PN24P. J.D. Richardson was supported under NASA contract 959203
from the JPL to MIT. McClanahan and S. Kramer carried out the processing
of the data. The zero-offset tables were computed by D. Berdichevsky
using magnetic field rolls calibrations and "z axis calibration." We
thank Edward Stone and his coinvestigators on the CRS experiment on V2
for making their data available for distribution on COHOweb.
NR 32
TC 1
Z9 1
U1 1
U2 3
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 AUG
PY 2014
VL 119
IS 8
DI 10.1002/2014JA020297
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AT3BJ
UT WOS:000344809600004
ER
PT J
AU Collinson, GA
Fedorov, A
Futaana, Y
Masunaga, K
Hartle, R
Stenberg, G
Grebowsky, J
Holmstrom, M
Andre, N
Barabash, S
Zhang, TL
AF Collinson, G. A.
Fedorov, A.
Futaana, Y.
Masunaga, K.
Hartle, R.
Stenberg, G.
Grebowsky, J.
Holmstrom, M.
Andre, N.
Barabash, S.
Zhang, T. L.
TI The extension of ionospheric holes into the tail of Venus
SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS
LA English
DT Article
ID MAGNETIC-FIELDS; EXPRESS MISSION; SPACE PLASMAS; NIGHTSIDE; ANALYZER;
ASPERA-4; FLOW; WAKE
AB Ionospheric holes are Cytherian nightside phenomena discovered by the NASA Pioneer Venus Orbiter, featuring localized plasma depletions driven by prominent and unexplained enhancements in the draped interplanetary magnetic field. Observed only during solar maximum, the phenomenon remains unexplained, despite their frequent observation during the first 3 years of the mission and more than 30 years having elapsed since their first description in the literature. We present new observations by the European Space Agency Venus Express showing that ionospheric holes can extend much further into the tail than previously anticipated (1.2 to 2.4 planetary radii) and may be observed throughout the solar cycle and over a wide range of solar wind conditions. We find that ionospheric holes are a manifestation of a deeper underlying phenomenon: tubes of enhanced draped interplanetary magnetic field that emerge in pairs from below the ionosphere and stretch far down the tail. We speculate on two possible explanations for the magnetic fields underlying the phenomena: magnetic pileup due to stagnation of ionospheric flow and internal draping around a metallic core.
C1 [Collinson, G. A.; Hartle, R.; Grebowsky, J.] NASA, Heliophys Sci Div, Goddard Spaceflight Ctr, Greenbelt, MD 20771 USA.
[Collinson, G. A.; Futaana, Y.; Masunaga, K.; Stenberg, G.; Holmstrom, M.; Barabash, S.] Swedish Inst Space Phys, Inst Rymdfys, S-98128 Kiruna, Sweden.
[Collinson, G. A.] Catholic Univ Amer, Inst Astrophys & Computat Sci, Washington, DC 20064 USA.
[Fedorov, A.; Andre, N.] Univ Toulouse, Inst Rech Astrophys & Planetol, Toulouse, France.
[Masunaga, K.] Tohoku Univ, Dept Geophys, Sendai, Miyagi 980, Japan.
[Zhang, T. L.] Austrian Acad Sci, Space Res Inst, A-8010 Graz, Austria.
RP Collinson, GA (reprint author), NASA, Heliophys Sci Div, Goddard Spaceflight Ctr, Greenbelt, MD 20771 USA.
EM glyn.a.collinson@nasa.gov
FU CNES
FX We would like to thank Martin Wieser for his support and CNES for a
travel grant which facilitated the survey. We also thank Elena Budnik
and the AMDA team, Robin Ramsted, Menelaos Sarantos, and Alex Young for
useful discussions. Venus Express data are available from the ESA
planetary science archive.
NR 38
TC 5
Z9 5
U1 1
U2 5
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 AUG
PY 2014
VL 119
IS 8
DI 10.1002/2014JA019851
PG 14
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AT3BJ
UT WOS:000344809600067
ER
PT J
AU Denton, RE
Takahashi, K
Thomsen, MF
Borovsky, JE
Singer, HJ
Wang, Y
Goldstein, J
Brandt, PC
Reinisch, BW
AF Denton, R. E.
Takahashi, K.
Thomsen, M. F.
Borovsky, J. E.
Singer, H. J.
Wang, Y.
Goldstein, J.
Brandt, P. C.
Reinisch, B. W.
TI Evolution of mass density and O plus concentration at geostationary
orbit during storm and quiet events
SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS
LA English
DT Article
ID INNER MAGNETOSPHERE; ELECTRON-DENSITIES; OUTER PLASMASPHERE; POLAR-CAP;
ART.; FIELD; PLASMAPAUSE; IONS; IONOSPHERE; DYNAMICS
AB We investigated mass density rho(m) and O+ concentration eta(O+) = n(O+)/n(e) (where n(O+) and n(e) are the O+ and electron density, respectively) during two events, one active and one more quiet. We found rho(m) from observations of Alfven wave frequencies measured by the GOES, and we investigated composition by combining measurements of rho(m) with measurements of ion density n(MPA, i) from the Magnetospheric Plasma Analyzer (MPA) instrument on Los Alamos National Laboratory spacecraft or n(e) from the Radio Plasma Imager instrument on the Imager forMagnetopause-to-Aurora Global Exploration spacecraft. Using a simple assumption for the He+ density at solar maximum based on a statistical study, we found eta(O+) values ranging from near zero to close to unity. For geostationary spacecraft that corotate with the Earth, sudden changes in density for both rho(m) and n(e) often appear between dusk and midnight magnetic local time, especially when Kp is significantly above zero. This probably indicates that the bulk (total) ions have energy below a few keV and that the satellites are crossing from closed or previously closed to open drift paths. During long periods that are geomagnetically quiet, the mass density varies little, but ne gradually refills leading to a gradual change in composition from low-density plasma that is relatively cold and heavy (high-average ion mass M = rho(m)/n(e)) to high-density plasma that is relatively cold and light (low M) plasmasphere-like plasma. During active periods we observe a similar daily oscillation in plasma properties from the dayside to the nightside, with cold and light high-density plasma (more plasmasphere-like) on the dayside and hotter and more heavy low-density plasma (more plasma sheet-like) on the nightside. The value of ne is very dependent on whether it is measured inside or outside a plasmaspheric plume, while rho(m) is not. All of our results were found at solar maximum; previous results suggest that there will be much less O+ at solar minimum under all conditions.
C1 [Denton, R. E.] Dartmouth Coll, Dept Phys & Astron, Hanover, NH 03755 USA.
[Takahashi, K.; Brandt, P. C.] Johns Hopkins Univ Appl Phys Lab, Laurel, MD USA.
[Thomsen, M. F.] Los Alamos Natl Lab, Los Alamos, NM USA.
[Borovsky, J. E.] Space Sci Inst, Boulder, CO USA.
[Singer, H. J.] Natl Ocean & Atmospher Adm Space Weather Predict, Boulder, CO USA.
[Wang, Y.] NASA Goddard Space Flight Ctr, Goddard Earth Sci & Technol Ctr, Greenbelt, MD USA.
[Wang, Y.] Univ Maryland Baltimore Cty, Baltimore, MD 21228 USA.
[Goldstein, J.] Southwest Res Inst, San Antonio, TX USA.
[Reinisch, B. W.] Univ Massachusetts Lowell, Space Sci Lab, Lowell, MA USA.
RP Denton, RE (reprint author), Dartmouth Coll, Dept Phys & Astron, Hanover, NH 03755 USA.
EM richard.e.denton@dartmouth.edu
RI Brandt, Pontus/N-1218-2016
OI Brandt, Pontus/0000-0002-4644-0306
FU NSF [AGS-1105790, ATM-0855924]; NASA [NNX10AQ60G, NNX11AO59G]
FX Work at Dartmouth College was supported by NSF grant AGS-1105790 and
NASA grants NNX10AQ60G (Living with a Star Targeted Research
Plasmasphere focused science topic) and NNX11AO59G (Heliophysics Theory
Program). Work at the Applied Physics Laboratory was supported by NSF
grant ATM-0855924. We thank the reviewers for helpful comments.
Supplementary materials for this paper include GOES magnetometer data,
calculated Alfven frequencies and mass density, and IMAGE RPI electron
density. Most LANL MPA data used in this study are available at CDAWeb.
NR 44
TC 4
Z9 4
U1 1
U2 7
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 AUG
PY 2014
VL 119
IS 8
DI 10.1002/2014JA019888
PG 15
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AT3BJ
UT WOS:000344809600028
ER
PT J
AU Fatemi, S
Holmstrom, M
Futaana, Y
Lue, C
Collier, MR
Barabash, S
Stenberg, G
AF Fatemi, Shahab
Holmstrom, Mats
Futaana, Yoshifumi
Lue, Charles
Collier, Michael R.
Barabash, Stas
Stenberg, Gabriella
TI Effects of protons reflected by lunar crustalmagnetic fields on the
global lunar plasma environment
SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS
LA English
DT Article
ID MONOCHROMATIC WHISTLER WAVES; SOLAR-WIND; MAGNETIC-FIELDS; BOW SHOCK;
ION-BEAM; WAKE; MOON; INSTABILITIES; SURFACE; KAGUYA
AB Solar wind plasma interaction with lunar crustal magnetic fields is different than that of magnetized bodies like the Earth. Lunar crustal fields are, for typical solar wind conditions, not strong enough to form a (bow) shock upstream but rather deflect and perturb plasma and fields. Here we study the global effects of protons reflected from lunar crustal magnetic fields on the lunar plasma environment when the Moon is in the unperturbed solar wind. We employ a three-dimensional hybrid model of plasma and an observed map of reflected protons from lunar magnetic anomalies over the lunar farside. We observe that magnetic fields and plasma upstream over the lunar crustal fields compress to nearly 120% and 160% of the solar wind, respectively. We find that these disturbances convect downstream in the vicinity of the lunar wake, while their relative magnitudes decrease. In addition, solar wind protons are disturbed and heated at compression regions and their velocity distribution changes from Maxwellian to a non-Maxwellian. Finally, we show that these features persists, independent of the details of the ion reflection by the magnetic fields.
C1 [Fatemi, Shahab; Holmstrom, Mats; Futaana, Yoshifumi; Lue, Charles; Barabash, Stas; Stenberg, Gabriella] Swedish Inst Space Phys, S-98128 Kiruna, Sweden.
[Fatemi, Shahab] Lulea Univ Technol, Div Space Technol, Dept Comp Sci Elect & Space Engn, S-95187 Lulea, Sweden.
[Lue, Charles] Umea Univ, Dept Phys, Umea, Sweden.
[Collier, Michael R.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Fatemi, S (reprint author), Swedish Inst Space Phys, S-98128 Kiruna, Sweden.
EM shahab@irf.se
RI Collier, Michael/I-4864-2013
OI Collier, Michael/0000-0001-9658-6605
FU National Graduate School of Space Technology (NGSST); Lulea University
of Technology; Swedish National Space Board (SNSB); National Graduate
School of Scientific Computing (NGSSC), Uppsala University, Sweden
FX The work of Shahab Fatemi was supported by the National Graduate School
of Space Technology (NGSST), Lulea University of Technology, the Swedish
National Space Board (SNSB), and the National Graduate School of
Scientific Computing (NGSSC), Uppsala University, Sweden. This research
was conducted using resources provided by the Swedish National
Infrastructure for Computing (SNIC) at the High Performance Computing
Center North (HPC2N), Umea University, Sweden. The software used in this
work was in part developed by the DOE NNSA-ASC OASCR Flash Center at the
University of Chicago. The authors thank the International Space Science
Institute (ISSI) Bern, Switzerland, for organizing a meeting when the
topic of this paper was extensively discussed. We thank the teams who
created and provided WIND magnetic field and plasma data used in this
analysis, including K. W. Ogilvie, A.J. Lazarus, and R. Lepping. The
authors also thank the reviewers for their valuable comments to improve
this manuscript.
NR 50
TC 10
Z9 10
U1 0
U2 5
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 AUG
PY 2014
VL 119
IS 8
DI 10.1002/2014JA019900
PG 11
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AT3BJ
UT WOS:000344809600006
ER
PT J
AU Feynman, J
Ruzmaikin, A
AF Feynman, J.
Ruzmaikin, A.
TI The Centennial Gleissberg Cycle and its association with extendedminima
SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS
LA English
DT Article
ID LONG-TERM VARIATION; MEAN-FIELD DYNAMO; SOLAR-WIND SPEED; DIFFERENTIAL
ROTATION; GEOMAGNETIC-ACTIVITY; INTERPLANETARY FIELD; STELLAR DYNAMOS;
MAGNETIC-FIELD; GRAND MINIMA; TIME SCALES
AB The recent extended minimum of solar and geomagnetic variability (XSM) mirrors the XSMs in the nineteenth and twentieth centuries: 1810-1830 and 1900-1910. Such extended minima also were evident in aurorae reported from 450 A. D. to 1450 A. D. This paper argues that these minima are consistent with minima of the Centennial Gleissberg Cycles (CGCs), a 90-100 year variation observed on the Sun, in the solar wind, at the Earth, and throughout the heliosphere. The occurrence of the recent XSM is consistent with the existence of the CGC as a quasiperiodic variation of the solar dynamo. Evidence of CGCs is provided by the multicentury sunspot record, by the almost 150 year record of indexes of geomagnetic activity (1868 to present), by 1000 years of observations of aurorae (from 450 to 1450 A. D.) and millennial records of radionuclides in ice cores. The aa index of geomagnetic activity carries information about the two components of the solar magnetic field (toroidal and poloidal), one driven by flares and coronal mass ejections (related to the toroidal field) and the other driven by corotating interaction regions in the solar wind (related to the poloidal field). These two components systematically vary in their intensity and relative phase giving us information about centennial changes of the sources of solar dynamo during the recent CGC over the last century. The dipole and quadrupole modes of the solar magnetic field changed in relative amplitude and phase; the quadrupole mode became more important as the XSM was approached. Some implications for the solar dynamo theory are discussed.
C1 [Feynman, J.; Ruzmaikin, A.] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
RP Ruzmaikin, A (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
EM alexander.ruzmaikin@jpl.nasa.gov
FU Jet Propulsion Laboratory of the California Institute of Technology
under National Aeronautics and Space Administration
FX We thank reviewers for helpful, critical comments. This work was
supported in part by the Jet Propulsion Laboratory of the California
Institute of Technology, under a contract with the National Aeronautics
and Space Administration.
NR 79
TC 4
Z9 4
U1 0
U2 4
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 AUG
PY 2014
VL 119
IS 8
DI 10.1002/2013JA019478
PG 15
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AT3BJ
UT WOS:000344809600002
ER
PT J
AU Raines, JM
Gershman, DJ
Slavin, JA
Zurbuchen, TH
Korth, H
Anderson, BJ
Solomon, SC
AF Raines, Jim M.
Gershman, Daniel J.
Slavin, James A.
Zurbuchen, Thomas H.
Korth, Haje
Anderson, Brian J.
Solomon, Sean C.
TI Structure and dynamics of Mercury'smagnetospheric cusp: MESSENGER
measurements of protons and planetary ions
SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS
LA English
DT Article
ID MAGNETOPAUSE RECONNECTION RATE; MONTE-CARLO MODEL; SOLAR-WIND;
MAGNETIC-FIELD; MERCURYS MAGNETOSPHERE; POLAR MAGNETOSPHERE; INNER
HELIOSPHERE; PLASMA; SURFACE; EXOSPHERE
AB The MErcury Surface, Space ENvironment, GEochemistry, and Ranging (MESSENGER) spacecraft has observed the northern magnetospheric cusp of Mercury regularly since the probe was inserted into orbit about the innermost planet in March 2011. Observations from the Fast Imaging Plasma Spectrometer (FIPS) made at altitudes < 400 km in the planet's cusp have shown average proton densities (> 10 cm(-3)) that are exceeded only by those observed in the magnetosheath. These high plasma densities are also associated with strong diamagnetic depressions observed by MESSENGER's Magnetometer. Plasma in the cusp may originate from several sources: (1) Direct inflow from the magnetosheath, (2) locally produced planetary photoions and ions sputtered off the surface from solar wind impact and then accelerated upward, and (3) flow of magnetosheath and magnetospheric plasma accelerated from dayside reconnection X-lines. We surveyed 518 cusp passes by MESSENGER, focusing on the spatial distribution, energy spectra, and pitch-angle distributions of protons and Na+-group ions. Of those, we selected 77 cusp passes during which substantial Na+-group ion populations were present for a more detailed analysis. We find that Mercury's cusp is a highly dynamic region, both in spatial extent and plasma composition and energies. From the three-dimensional plasma distributions observed by FIPS, protons with mean energies of 1 keV were found flowing down into the cusp (i.e., source (1) above). The distribution of pitch angles of these protons showed a depletion in the direction away from the surface, indicating that ions within 40 degrees of the magnetic field direction are in the loss cone, lost to the surface rather than being reflected by the magnetic field. In contrast, Na+-group ions show two distinct behaviors depending on their energy. Low-energy (100-300 eV) ions appear to be streaming out of the cusp, showing pitch-angle distributions with a strong component antiparallel to the magnetic field (away from the surface). These ions appear to have been generated in the cusp and accelerated locally (i.e., source (2) above). Higher-energy (>= 1keV) Na+-group ions in the cusp exhibit much larger perpendicular components in their energy distributions. During active times, as judged by frequent, large-amplitude magnetic field fluctuations, many more Na+-group ions are measured at latitudes south of the cusp. In several cases, these Na+-group ions in the dayside magnetosphere are flowing northward toward the cusp. The high mean energy, pitch-angle distributions, and large number of Na+-group ions on dayside magnetospheric field lines are inconsistent with direct transport into the cusp of sputtered ions from the surface or newly photoionized particles. Furthermore, the highest densities and mean energies often occur together with high-amplitude magnetic fluctuations, attributed to flux transfer events along the magnetopause. These results indicate that high-energy Na+-group ions in the cusp are likely formed by ionization of escaping neutral Na in the outer dayside magnetosphere and the magnetosheath followed by acceleration and transport into the cusp by reconnection at the subsolar magnetopause (i.e., source 3 above).
C1 [Raines, Jim M.; Gershman, Daniel J.; Slavin, James A.; Zurbuchen, Thomas H.] Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA.
[Gershman, Daniel J.] NASA Goddard Space Flight Ctr, Geospace Phys Lab, Greenbelt, MD USA.
[Korth, Haje; Anderson, Brian J.] Johns Hopkins Univ Appl Phys Lab, Laurel, MD USA.
[Solomon, Sean C.] Columbia Univ, Lamont Doherty Earth Observ, Palisades, NY USA.
[Solomon, Sean C.] Carnegie Inst Sci, Dept Terr Magnetism, Washington, DE USA.
RP Raines, JM (reprint author), Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA.
EM jraines@umich.edu
RI Slavin, James/H-3170-2012
OI Slavin, James/0000-0002-9206-724X
FU NASA Discovery Program [NAS5-97271, NASW-00002]
FX 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.
J.M.R. thanks D. Schriver and T. A. Cassidy for discussions helpful to
this work. Data used in this study are available from the Planetary Data
System.
NR 59
TC 22
Z9 22
U1 1
U2 6
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 AUG
PY 2014
VL 119
IS 8
DI 10.1002/2014JA020120
PG 16
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AT3BJ
UT WOS:000344809600039
ER
PT J
AU Selesnick, RS
Baker, DN
Jaynes, AN
Li, X
Kanekal, SG
Hudson, MK
Kress, BT
AF Selesnick, R. S.
Baker, D. N.
Jaynes, A. N.
Li, X.
Kanekal, S. G.
Hudson, M. K.
Kress, B. T.
TI Observations of the inner radiation belt: CRAND and trapped solar
protons
SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS
LA English
DT Article
ID ENERGY; ZONE
AB Measurements of inner radiation belt protons have been made by the Van Allen Probes Relativistic Electron-Proton Telescopes as a function of kinetic energy (24 to 76 MeV), equatorial pitch angle, and magnetic L shell, during late 2013 and early 2014. A probabilistic data analysis method reduces background from contamination by higher-energy protons. Resulting proton intensities are compared to predictions of a theoretical radiation belt model. Then trapped protons originating both from cosmic ray albedo neutron decay (CRAND) and from trapping of solar protons are evident in the measured distributions. An observed double-peaked distribution in L is attributed, based on the model comparison, to a gap in the occurrence of solar proton events during the 2007 to 2011 solar minimum. Equatorial pitch angle distributions show that trapped solar protons are confined near the magnetic equator but that CRAND protons can reach low altitudes. Narrow pitch angle distributions near the outer edge of the inner belt are characteristic of proton trapping limits.
C1 [Selesnick, R. S.] Air Force Res Lab, Space Vehicles Directorate, Kirtland AFB, NM USA.
[Baker, D. N.; Jaynes, A. N.; Li, X.] Univ Colorado, Lab Atmospher & Space Phys, Boulder, CO 80309 USA.
[Li, X.] Univ Colorado, Dept Aerosp Engn Sci, Boulder, CO 80309 USA.
[Kanekal, S. G.] NASA Goddard Space Flight Ctr, Greenbelt, MD USA.
[Hudson, M. K.; Kress, B. T.] Dartmouth Coll, Dept Phys & Astron, Hanover, NH 03755 USA.
RP Selesnick, RS (reprint author), Air Force Res Lab, Space Vehicles Directorate, Kirtland AFB, NM USA.
EM richard.selesnick@us.af.mil
FU NASA [NNH14AX18I]; Air Force Research Laboratory under the Heliophysics
Guest Investigators Program, at University of Colorado; College by
RBSP-ECT through JHU/APL under prime NASA [967399, NAS5-01072]; NSF
[ATM-1023332]
FX The authors thank C. A. Kletzing for EMFISIS magnetic field data used in
pitch angle determination and M. G. Henderson and G. D. Reeves for
magnetic ephemeris data from the IGRF+OP77Q model. Van Allen Probes REPT
and ephemeris data are available from the ECT Science Operations and
Data Center, http://www.rbsp-ect.lanl.gov, and EMFISIS data from
http://emfisis.physics.uiowa.edu. This work was supported in part by
NASA agreement NNH14AX18I with the Air Force Research Laboratory under
the Heliophysics Guest Investigators Program, at University of Colorado
and Dartmouth College by RBSP-ECT funding through JHU/APL contract
967399 under prime NASA contract NAS5-01072, and by NSF grant
ATM-1023332 to Dartmouth College.
NR 21
TC 11
Z9 11
U1 0
U2 6
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 AUG
PY 2014
VL 119
IS 8
DI 10.1002/2014JA020188
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AT3BJ
UT WOS:000344809600035
ER
PT J
AU Voros, Z
Facsko, G
Khodachenko, M
Honkonen, I
Janhunen, P
Palmroth, M
AF Voeroes, Z.
Facsko, G.
Khodachenko, M.
Honkonen, I.
Janhunen, P.
Palmroth, M.
TI Windsock memory COnditioned RAM (CO-RAM) pressure effect: Forced
reconnection in the Earth's magnetotail
SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS
LA English
DT Article
ID INTERPLANETARY MAGNETIC-FIELD; SOLAR-WIND; PLASMA SHEET; MAGNETOSPHERE;
CLUSTER; INSTRUMENT; SUBSTORMS; TAIL; IMF; IDENTIFICATION
AB Magnetic reconnection (MR) is a key physical concept explaining the addition of magnetic flux to the magnetotail and closed flux lines back-motion to the dayside magnetosphere. This scenario elaborated by Dungey (1963) can explain many aspects of solar wind-magnetosphere interaction processes, including substorms. However, neither the Dungey model nor its numerous modifications were able to explain fully the onset conditions for MR in the tail. In this paper, we introduce new onset conditions for forced MR in the tail. We call our scenario the "windsock memory conditioned ram pressure effect." Our nonflux transfer-associated forcing is introduced by a combination of the large-scale windsock motions exhibiting memory effects and solar wind dynamic pressure actions on the nightside magnetopause during northward oriented interplanetary magnetic field (IMF). Using global MHD Grand Unified Magnetosphere Ionosphere Coupling Simulation version 4 simulation results, upstream data from Wind, magnetosheath data from Cluster 1 and distant tail data from the two-probe Acceleration, Reconnection, Turbulence and Electrodynamics of the Moon's Interaction with the Sun mission, we show that the simultaneous occurrence of vertical windsock motions of the magnetotail and enhanced solar wind dynamic pressure introduces strong nightside disturbances, including enhanced electric fields and persistent vertical cross-tail shear flows. These perturbations, associated with a stream interaction region in the solar wind, drive MR in the tail during episodes of northward oriented interplanetary magnetic field (IMF). We detect MR indirectly, observing plasmoids in the tail and ground-based signatures of earthward moving fast flows. We also consider the application to solar system planets and close-in exoplanets, where the proposed scenario can elucidate some new aspects of solar/stellar wind-magnetosphere interactions.
C1 [Voeroes, Z.; Khodachenko, M.] Austrian Acad Sci, Space Res Inst, A-8010 Graz, Austria.
[Voeroes, Z.] Univ Innsbruck, Inst Astro & Particle Phys, A-6020 Innsbruck, Austria.
[Facsko, G.] Hungarian Acad Sci, Geodet & Geophys Inst, Res Ctr Astron & Earth Sci, Sopron, Hungary.
[Facsko, G.; Honkonen, I.; Janhunen, P.; Palmroth, M.] Finnish Meteorol Inst, FIN-00101 Helsinki, Finland.
[Khodachenko, M.] Moscow MV Lomonosov State Univ, Skobeltsyn Inst Nucl Phys, Moscow, Russia.
[Honkonen, I.] NASA GSFC, Greenbelt, MD USA.
RP Voros, Z (reprint author), Austrian Acad Sci, Space Res Inst, A-8010 Graz, Austria.
EM zoltan.voeroes@oeaw.ac.at
OI Voros, Zoltan/0000-0001-7597-238X
FU Austrian Fond zur Forderung der wissenschaftlichen Forschung
[P24740-N27, S11606-N16, Y398]; European Research Council under the
European Community [200141-QuESpace]; ECLAT FP7 [263325]; OTKA of the
Hungarian Scientific Research Fund [K75640]; NASA [NAS5-02099]
FX The authors would like to thank A. Runov (UCLA, Los Angeles, USA); R.
Nakamura, M. Panchenko, M. Volwerk, and T. L. Zhang (IWF, Graz Austria);
Ch.J. Owen (MSSL, London, UK); J. Borovsky (University of Michigan,
USA); and A. Kendl (University of Innsbruck, Austria) for very useful
discussions and support. This work was supported by the Austrian Fond
zur Forderung der wissenschaftlichen Forschung (projects P24740-N27,
S11606-N16, and Y398). Part of the research has received funding from
the European Research Council under the European Communitys Seventh
Framework Programme (FP7/2007-2013)/ERC Starting grant 200141-QuESpace
and from ECLAT FP7 grant 263325. Gabor Facsko was also supported by the
OTKA grant K75640 of the Hungarian Scientific Research Fund. We
acknowledge NASA contract NAS5-02099 and V. Angelopoulos for the use of
data from the THEMIS/ARTEMIS mission. We acknowledge the use of Kyoto
WDC AE index and geomagnetic observatory data from IQA (Canada), SKT,
GHB, FHB, NAQ, and AMK (Greenland). Figure 1 was created by the
Satellite Situation Center 4-D Orbit Viewer. The GUMICS-4 model
developed at FMI represents a part of the computational modeling
infrastructure of the EU FP7 project IMPEX
(http://impex-FP7.oeaw.ac.at).
NR 69
TC 4
Z9 4
U1 0
U2 12
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 AUG
PY 2014
VL 119
IS 8
DI 10.1002/2014JA019857
PG 21
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AT3BJ
UT WOS:000344809600019
ER
PT J
AU Wilson, LB
Sibeck, DG
Breneman, AW
Le Contel, O
Cully, C
Turner, DL
Angelopoulos, V
Malaspina, DM
AF Wilson, L. B., III
Sibeck, D. G.
Breneman, A. W.
Le Contel, O.
Cully, C.
Turner, D. L.
Angelopoulos, V.
Malaspina, D. M.
TI Quantified energy dissipation rates in the terrestrial bow shock: 2.
Waves and dissipation
SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS
LA English
DT Article
ID ELECTROSTATIC SOLITARY WAVES; CYCLOTRON DRIFT INSTABILITY;
QUASI-PERPENDICULAR SHOCK; HIGH MACH NUMBER; FAST MODE SHOCKS;
PLASMA-WAVES; SOLAR-WIND; ANOMALOUS RESISTIVITY; NONLINEAR EVOLUTION;
BEAM INSTABILITIES
AB We present the first quantified measure of the energy dissipation rates, due to wave-particle interactions, in the transition region of the Earth's collisionless bow shock using data from the Time History of Events and Macroscale Interactions during Substorms spacecraft. Our results show that wave-particle interactions can regulate the global structure and dominate the energy dissipation of collisionless shocks. In every bow shock crossing examined, we observed both low-frequency (< 10 Hz) and high-frequency (greater than or similar to 10 Hz) electromagnetic waves throughout the entire transition region and into the magnetosheath. The low-frequency waves were consistent with magnetosonic-whistler waves. The high-frequency waves were combinations of ion-acoustic waves, electron cyclotron drift instability driven waves, electrostatic solitary waves, and whistler mode waves. The high-frequency waves had the following: (1) peak amplitudes exceeding delta B similar to 10 nT and delta E similar to 300 mV/m, though more typical values were delta B similar to 0.1-1.0 nT and delta B similar to 10-50 mV/m; (2) Poynting fluxes in excess of 2000 mu Wm(-2) (typical values were similar to 1-10 mu W m(-2)); (3) resistivities > 9000 Omega m; and (4) associated energy dissipation rates > 10 mu Wm(-3). The dissipation rates due to wave-particle interactions exceeded rates necessary to explain the increase in entropy across the shock ramps for similar to 90% of the wave burst durations. For similar to 22% of these times, the wave-particle interactions needed to only be = 0.1% efficient to balance the nonlinear wave steepening that produced the shock waves. These results show that wave-particle interactions have the capacity to regulate the global structure and dominate the energy dissipation of collisionless shocks.
C1 [Wilson, L. B., III; Sibeck, D. G.] NASA Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Breneman, A. W.] Univ Minnesota, Sch Phys & Astron, Minneapolis, MN 55455 USA.
[Le Contel, O.] Ecole Polytech, Lab Phys Plasmas, Palaiseau, France.
[Cully, C.] Univ Calgary, Dept Phys & Astron, Calgary, AB T2N 1N4, Canada.
[Turner, D. L.; Angelopoulos, V.] Univ Calif Los Angeles, Inst Geophys & Planetary Phys Earth & Space Sci, Los Angeles, CA USA.
[Malaspina, D. M.] Univ Colorado, Inst Geophys & Planetary Phys Earth & Space Sci, Boulder, CO 80309 USA.
RP Wilson, LB (reprint author), NASA Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
EM lynn.b.wilsoniii@gmail.com
RI Wilson III, Lynn/D-4425-2012; Cully, Christopher/P-2539-2016
OI Wilson III, Lynn/0000-0002-4313-1970;
FU Wind MODA grants; CNES; CNRS-INSU
FX We would like to thank A.F.-Vinas, D. Bryant, D. A. Roberts, R. T.
Wicks, R. Lysak, and M. L. Goldstein for useful discussions of the
fundamental physics involved in our study. The work was partially
supported by Wind MO&DA grants. The French involvement (SCM instruments)
on THEMIS are supported by CNES and CNRS-INSU. The data used in this
paper and the associated calibration software can be found at
http://themis.ssl.berkeley.edu/index.shtml.
NR 103
TC 7
Z9 7
U1 1
U2 9
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 AUG
PY 2014
VL 119
IS 8
DI 10.1002/2014JA019930
PG 21
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AT3BJ
UT WOS:000344809600032
ER
PT J
AU Wilson, LB
Sibeck, DG
Breneman, AW
Le Contel, O
Cully, C
Turner, DL
Angelopoulos, V
Malaspina, DM
AF Wilson, L. B., III
Sibeck, D. G.
Breneman, A. W.
Le Contel, O.
Cully, C.
Turner, D. L.
Angelopoulos, V.
Malaspina, D. M.
TI Quantified energy dissipation rates in the terrestrial bow shock: 1.
Analysis techniques and methodology
SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS
LA English
DT Article
ID QUASI-PERPENDICULAR SHOCKS; PHASE-SPACE SIGNATURES; ELECTRON CROSS-TALK;
HIGH MACH NUMBER; HIGH-BETA; ISEE-2 OBSERVATIONS; RESOLVED LAYER;
ELECTROMAGNETIC-WAVES; ANOMALOUS RESISTIVITY; ION DISTRIBUTIONS
AB We present a detailed outline and discussion of the analysis techniques used to compare the relevance of different energy dissipation mechanisms at collisionless shock waves. We show that the low-frequency, quasi-static fields contribute less to ohmic energy dissipation, (-j.E), than their high-frequency counterparts. In fact, we found that high-frequency, large-amplitude (>100 mV/m and/or >1 nT) waves are ubiquitous in the transition region of collisionless shocks. We quantitatively show that their fields, through wave-particle interactions, cause enough energy dissipation to regulate the global structure of collisionless shocks. The purpose of this paper, part one of two, is to outline and describe in detail the background, analysis techniques, and theoretical motivation for our new results presented in the companion paper. The companion paper presents the results of our quantitative energy dissipation rate estimates and discusses the implications. Together, the two manuscripts present the first study quantifying the contribution that high-frequency waves provide, through wave-particle interactions, to the total energy dissipation budget of collisionless shock waves.
C1 [Wilson, L. B., III; Sibeck, D. G.] NASA Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Breneman, A. W.] Univ Minnesota, Sch Phys & Astron, Minneapolis, MN 55455 USA.
[Le Contel, O.] Ecole Polytech, Lab Phys Plasmas, Palaiseau, France.
[Cully, C.] Univ Calgary, Dept Phys & Astron, Calgary, AB T2N 1N4, Canada.
[Turner, D. L.; Angelopoulos, V.] Univ Calif Los Angeles, Inst Geophys & Planetary Phys Earth & Space Sci, Los Angeles, CA USA.
[Malaspina, D. M.] Univ Colorado, Lab Atmospher & Space Phys, Boulder, CO 80309 USA.
RP Wilson, LB (reprint author), NASA Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
EM lynn.b.wilsoniii@gmail.com
RI Wilson III, Lynn/D-4425-2012; Cully, Christopher/P-2539-2016
OI Wilson III, Lynn/0000-0002-4313-1970;
FU Wind MO grant; Wind DA grant; CNES; CNRS-INSU
FX We would like to thank A.F.-Vinas, D. Bryant, D. A. Roberts, R. T.
Wicks, R. Lysak, and M. L. Goldstein for useful discussions of the
fundamental physics involved in our study. The work was partially
supported by Wind MO and DA grants. The French involvement (SCM
instruments) on THEMIS are supported by CNES and CNRS-INSU. The data
used in this paper and the associated calibration software can be found
at http://themis.ssl.berkeley.edu/index.shtml.
NR 87
TC 5
Z9 5
U1 2
U2 12
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 AUG
PY 2014
VL 119
IS 8
DI 10.1002/2014JA019929
PG 20
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AT3BJ
UT WOS:000344809600031
ER
PT J
AU Mikouchi, T
Komatsu, M
Hagiya, K
Ohsumi, K
Zolensky, ME
Hoffmann, V
Martinez, J
Hochleitner, R
Kaliwoda, M
Terada, Y
Yagi, N
Takata, M
Satake, W
Aoyagi, Y
Takenouchi, A
Karouji, Y
Uesugi, M
Yada, T
AF Mikouchi, Takashi
Komatsu, Mutsumi
Hagiya, Kenji
Ohsumi, Kazumasa
Zolensky, Michael E.
Hoffmann, Viktor
Martinez, James
Hochleitner, Rupert
Kaliwoda, Melanie
Terada, Yasuko
Yagi, Naoto
Takata, Masaki
Satake, Wataru
Aoyagi, Yuya
Takenouchi, Atsushi
Karouji, Yuzuru
Uesugi, Masayuki
Yada, Toru
TI Mineralogy and crystallography of some Itokawa particles returned by the
Hayabusa asteroidal sample return mission
SO EARTH PLANETS AND SPACE
LA English
DT Article
DE Itokawa; Hayabusa; Olivine; Plagioclase; SR-XRD; SR-XANES; LL chondrites
ID ALMAHATA SITTA UREILITE; ORDINARY CHONDRITES; DUST PARTICLES; 2008 TC3;
BRECCIA; REGOLITH; PYROXENE; HISTORY
AB We studied seven Itokawa particles provided by the Japan Aerospace Exploration Agency (JAXA) as first International Announcement of Opportunity (AO) study mainly using electron and synchrotron radiation X-ray beam techniques. All the analyzed particles were collected from the first-touchdown site and composed of olivine and plagioclase with traces of Ca phosphate and chromite, and do not contain pyroxenes. Optical microscopy of these particles shows minor undulatory extinction of olivine and plagioclase, suggesting minor shock metamorphism (shock stage: S2). The electron microprobe analysis shows that olivine is Fo(70-73) and plagioclase is An(13-10)Or(5-7). The synchrotron radiation X-ray diffraction (SR-XRD) analysis of olivine crystals gives cell dimensions of a = 4.708 to 4.779 angstrom, b = 10.271 to 10.289 angstrom, c = 6.017 to 6.024 angstrom, corresponding to the Fo content of Fo(similar to 70) by Vegard's law. This composition matches the result obtained by the electron microprobe analysis. The olivine compositions of the analyzed particles are consistent with those of LL chondrites. The cell dimensions of two plagioclase crystals (a = 8.180 to 8.194 angstrom, b = 12.53 to 12.893 angstrom, c = 7.125 to 7.23 angstrom, a = 92.6 degrees to 93.00 degrees, beta = 116.36 degrees to 116.75 degrees, gamma = 90.03 degrees to 90.17 degrees) indicate that their equilibration temperatures are 800 degrees C +/- 10 degrees C. This temperature is near the peak metamorphic temperature recorded by equilibrated ordinary chondrites. The size of plagioclase crystals and the homogeneity of olivine compositions indicate that their petrologic type is >= 5. We also analyzed plagioclase by SR iron X-ray absorption near-edge structure (SR-XANES) and found that its Fe3+/(Fe2+ + Fe3+) ratio is approximately 0.5. Such high Fe3+ abundance indicates the formation under a relatively oxidizing environment. Thus, all these analyses have reconfirmed that the Itokawa particles returned by the Hayabusa spacecraft are very weakly shocked equilibrated LL chondrites, which matches the results of the preliminary examination team.
C1 [Mikouchi, Takashi; Satake, Wataru; Aoyagi, Yuya; Takenouchi, Atsushi] Univ Tokyo, Grad Sch Sci, Dept Earth & Planetary Sci, Bunkyo Ku, Tokyo 1130033, Japan.
[Komatsu, Mutsumi] Waseda Univ, Waseda Inst Adv Study, Shinjuku Ku, Tokyo 1698050, Japan.
[Hagiya, Kenji] Univ Hyogo, Sch Sci, Kamigori, Hyogo 6781297, Japan.
[Ohsumi, Kazumasa; Terada, Yasuko; Yagi, Naoto; Takata, Masaki] Japan Synchrotron Radiat Res Inst JASRI, Sayo, Hyogo 6795198, Japan.
[Zolensky, Michael E.] NASA Johnson Space Ctr, Houston, TX 77058 USA.
[Hoffmann, Viktor] Univ Munich LMU, Sect Geophys, Dept Earth & Environm Sci, D-80333 Munich, Germany.
[Hoffmann, Viktor] Univ Tubingen, Dept Geosci, D-72074 Tubingen, Germany.
[Martinez, James] ESCG Jacobs, Houston, TX 77058 USA.
[Hochleitner, Rupert; Kaliwoda, Melanie] Mineral State Collect, D-80333 Munich, Germany.
[Karouji, Yuzuru; Uesugi, Masayuki; Yada, Toru] Japan Aerosp Explorat Agcy, Inst Space & Astronaut Sci, Chuo Ku, Sagamihara, Kanagawa 2525210, Japan.
RP Mikouchi, T (reprint author), Univ Tokyo, Grad Sch Sci, Dept Earth & Planetary Sci, Bunkyo Ku, 7-3-1 Hongo, Tokyo 1130033, Japan.
EM mikouchi@eps.s.u-tokyo.ac.jp
FU Japanese Ministry of Education, Culture, Sports, Science and Technology
[23360333]; SPring-8 long-term project [2010B1415]; KEK [2012G652];
NASA's Muses-C Program
FX We thank JAXA for providing us with the Itokawa particles. Advice for
the sample preparation and discussion with Dr. T. Nakamura was very
helpful. We are grateful for the constructive reviews by Drs. A.
Bischoff and T. Nakamura, and editorial handling by Dr. T. Okada. The
electron microscopy was performed at the Electron Microbeam Analysis
Facility for Mineralogy at the Department of Earth and Planetary
Science, University of Tokyo. A part of this study was supported by the
Grant-in-Aid for Scientific Research (B) by the Japanese Ministry of
Education, Culture, Sports, Science and Technology No. 23360333 (TM).
The SR-XRD work was supported by the SPring-8 long-term project
(2010B1415) and SR-XANES work was by KEK 2012G652. MEZ was supported by
NASA's Muses-C Program.
NR 31
TC 6
Z9 6
U1 1
U2 6
PU SPRINGER HEIDELBERG
PI HEIDELBERG
PA TIERGARTENSTRASSE 17, D-69121 HEIDELBERG, GERMANY
SN 1880-5981
J9 EARTH PLANETS SPACE
JI Earth Planets Space
PD AUG 1
PY 2014
VL 66
AR 82
DI 10.1186/1880-5981-66-82
PG 9
WC Geosciences, Multidisciplinary
SC Geology
GA AQ9XS
UT WOS:000343213300002
ER
PT J
AU Price, E
Mielikainen, J
Huang, ML
Huang, BM
Huang, HLA
Lee, T
AF Price, Erik
Mielikainen, Jarno
Huang, Melin
Huang, Bormin
Huang, Hung-Lung Allen
Lee, Tsengdar
TI GPU-Accelerated Longwave Radiation Scheme of the Rapid Radiative
Transfer Model for General Circulation Models (RRTMG)
SO IEEE JOURNAL OF SELECTED TOPICS IN APPLIED EARTH OBSERVATIONS AND REMOTE
SENSING
LA English
DT Article
DE Compute unified device architecture (CUDA); graphics processing unit
(GPU); RRTMG_LW; radiative transfer; weather research and forecasting
(WRF)
ID ATMOSPHERIC SOUNDING INTERFEROMETER; CLIMATE MODELS; COOLING RATES;
FLUXES
AB Atmospheric radiative transfer models calculate radiative transfer of electromagnetic radiation through a planetary atmosphere. One of such models is the rapid radiative transfer model (RRTM), which evaluates longwave and shortwave atmospheric radiative fluxes and heating rates. The RRTM for general circulation models (GCMs), RRTMG, is an accelerated version based on the single-column reference of RRTM. The longwave radiation scheme of RRTM for GCMs (RRTMG_LW) is one model that utilizes the correlated-k approach to calculate longwave fluxes and heating rates for application to GCMs. In this paper, the feasibility of using graphics processing units (GPUs) to accelerate the RRTMG_LW in weather research and forecasting (WRF) model is examined. GPUs allow a substantial performance improvement in RRTMG_LW with a large number of parallel compute cores at low cost and power. Our GPU version of RRTMG_LW yields the bit-exact outputs as its original Fortran code. Our results show that NVIDIA's K40 GPU achieves a speedup of 127x as compared to its CPU counterpart running on one CPU core of Intel Xeon E5-2603, whereas the speedup for one CPU socket (4 cores) of the Xeon E5-2603 with respect to one CPU core is only : 3.2x.
C1 [Price, Erik; Mielikainen, Jarno; Huang, Melin; Huang, Bormin; Huang, Hung-Lung Allen] Univ Wisconsin, Space Sci & Engn Ctr, Madison, WI 53706 USA.
[Lee, Tsengdar] NASA Headquarters, Washington, DC 20546 USA.
RP Huang, BM (reprint author), Univ Wisconsin, Space Sci & Engn Ctr, Madison, WI 53706 USA.
EM Bormin.Huang@ssec.wisc.edu
FU National Aeronautics and Space Administration (NASA) [NNX11AL83G]
FX This work was supported by the National Aeronautics and Space
Administration (NASA) under Grant NNX11AL83G. (Corresponding author: B.
Huang.)
NR 43
TC 6
Z9 6
U1 1
U2 13
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 AUG
PY 2014
VL 7
IS 8
BP 3660
EP 3667
DI 10.1109/JSTARS.2014.2315771
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 AQ8DZ
UT WOS:000343055200045
ER
PT J
AU Brzostek, ER
Fisher, JB
Phillips, RP
AF Brzostek, Edward R.
Fisher, Joshua B.
Phillips, Richard P.
TI Modeling the carbon cost of plant nitrogen acquisition: Mycorrhizal
trade-offs and multipath resistance uptake improve predictions of
retranslocation
SO JOURNAL OF GEOPHYSICAL RESEARCH-BIOGEOSCIENCES
LA English
DT Article
DE terrestrial biosphere models; retranslocation; nitrogen cycling;
mycorrhizae; plant carbon allocation; FUN model
ID NORTHERN HARDWOOD FOREST; NUTRIENT USE EFFICIENCY; ELEVATED CO2;
TEMPERATE FOREST; ECOSYSTEM PRODUCTIVITY; TERRESTRIAL ECOSYSTEMS;
ECTOMYCORRHIZAL FUNGI; ARBUSCULAR MYCORRHIZA; DEPOSITION GRADIENT;
SENESCING LEAVES
AB Accurate projections of the future land carbon (C) sink by terrestrial biosphere models depend on how nutrient constraints on net primary production are represented. While nutrient limitation is nearly universal, current models do not have a C cost for plant nutrient acquisition. Also missing are symbiotic mycorrhizal fungi, which can consume up to 20% of net primary production and supply up to 50% of a plant's nitrogen (N) uptake. Here we integrate simultaneous uptake and mycorrhizae into a cutting-edge plant N modelFixation and Uptake of Nitrogen (FUN)that can be coupled into terrestrial biosphere models. The C cost of N acquisition varies as a function of mycorrhizal type, with plants that support arbuscular mycorrhizae benefiting when N is relatively abundant and plants that support ectomycorrhizae benefiting when N is strongly limiting. Across six temperate forested sites (representing arbuscular mycorrhizal- and ectomycorrhizal-dominated stands and 176 site years), including multipath resistance improved the partitioning of N uptake between aboveground and belowground sources. Integrating mycorrhizae led to further improvements in predictions of N uptake from soil (R-2=0.69 increased to R-2=0.96) and from senescing leaves (R-2=0.29 increased to R-2=0.73) relative to the original model. On average, 5% and 9% of net primary production in arbuscular mycorrhizal- and ectomycorrhizal-dominated forests, respectively, was needed to support mycorrhizal-mediated acquisition of N. To the extent that resource constraints to net primary production are governed by similar trade-offs across all terrestrial ecosystems, integrating these improvements to FUN into terrestrial biosphere models should enhance predictions of the future land C sink.
C1 [Brzostek, Edward R.; Phillips, Richard P.] Indiana Univ, Dept Biol, Bloomington, IN 47405 USA.
[Fisher, Joshua B.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Fisher, Joshua B.] Univ Calif Los Angeles, Joint Inst Reg Earth Syst Sci & Engn, Los Angeles, CA USA.
RP Brzostek, ER (reprint author), Indiana Univ, Dept Biol, Bloomington, IN 47405 USA.
EM edbrzost@indiana.edu
OI Fisher, Joshua/0000-0003-4734-9085
FU U.S. Department of Energy-Office of Biological and Environmental
Research-Terrestrial Ecosystem Science Program [ER65415]; U.S. National
Science Foundation Ecosystem Science Program; National Aeronautics and
Space Administration
FX The model input and output data are included as Appendix S2 in the
supporting information. Funding was provided by the U.S. Department of
Energy-Office of Biological and Environmental Research-Terrestrial
Ecosystem Science Program (award ER65415) and by the U.S. National
Science Foundation Ecosystem Science Program. We would like to
acknowledge the researchers whose efforts to produce high-quality carbon
and nitrogen budgets across forested ecosystems allowed us to validate
the improvements to the model. We also thank M. Shi for the valuable
comments on the structure of the model. J.B.F. carried out the research
at the Jet Propulsion Laboratory, California Institute of Technology,
under a contract with the National Aeronautics and Space Administration
and at the Joint Institute for Regional Earth System Science and
Engineering, University of California at Los Angeles.
NR 89
TC 8
Z9 8
U1 5
U2 70
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 AUG
PY 2014
VL 119
IS 8
BP 1684
EP 1697
DI 10.1002/2014JG002660
PG 14
WC Environmental Sciences; Geosciences, Multidisciplinary
SC Environmental Sciences & Ecology; Geology
GA AQ7KK
UT WOS:000342993200013
ER
PT J
AU Zak, M
AF Zak, Michail
TI Interference of probabilities in dynamics
SO AIP ADVANCES
LA English
DT Article
AB A new class of dynamical systems with a preset type of interference of probabilities is introduced. It is obtained from the extension of the Madelung equation by replacing the quantum potential with a specially selected feedback from the Liouville equation. It has been proved that these systems are different from both Newtonian and quantum systems, but they can be useful for modeling spontaneous collective novelty phenomena when emerging outputs are qualitatively different from the weighted sum of individual inputs. Formation of language and fast decision-making process as potential applications of the probability interference is discussed. (C) 2014 Author(s).
C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Zak, M (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM michail.zak@gmail.com
NR 5
TC 0
Z9 0
U1 0
U2 0
PU AMER INST PHYSICS
PI MELVILLE
PA CIRCULATION & FULFILLMENT DIV, 2 HUNTINGTON QUADRANGLE, STE 1 N O 1,
MELVILLE, NY 11747-4501 USA
SN 2158-3226
J9 AIP ADV
JI AIP Adv.
PD AUG
PY 2014
VL 4
IS 8
AR 087130
DI 10.1063/1.4893871
PG 13
WC Nanoscience & Nanotechnology; Materials Science, Multidisciplinary;
Physics, Applied
SC Science & Technology - Other Topics; Materials Science; Physics
GA AQ4YX
UT WOS:000342808900030
ER
PT J
AU Kim, J
Rim, T
Lee, J
Baek, CK
Meyyappan, M
Lee, JS
AF Kim, Jungsik
Rim, Taiuk
Lee, Junyoung
Baek, Chang-Ki
Meyyappan, Meyya
Lee, Jeong-Soo
TI Threshold Voltage Variations Due to Oblique Single Grain Boundary in
Sub-50-nm Polysilicon Channel
SO IEEE TRANSACTIONS ON ELECTRON DEVICES
LA English
DT Article
DE Grain boundary (GB); poly-silicon (poly-Si) channel; threshold voltage
variation
ID THIN-FILM TRANSISTORS; DEPENDENCE; LOCATION; SIZE
AB We investigate the effect of single grain boundary (SGB) with arbitrary angles on the threshold voltage (V-th) variation in sub-50-nm polysilicon (poly-Si) channel devices using 3-D simulation. An SGB in the poly-Si channel causes changes in potential barrier profile resulting in the variation of V-th. As the planar devices scale down to 20-nm, oblique SGB can significantly increase the whole potential barrier profile and cause large V-th variation. However, due to superior gate controllability, the gate-all-around devices show relatively small increase of the conduction energy band, and thus mitigate the V-th variation even in 20-nm poly-Si channel.
C1 [Kim, Jungsik] Pohang Univ Sci & Technol, Div IT Convergence Engn, Pohang 790784, South Korea.
[Rim, Taiuk; Baek, Chang-Ki] Pohang Univ Sci & Technol, Dept Creat IT Engn, Pohang 790784, South Korea.
[Rim, Taiuk; Baek, Chang-Ki] Pohang Univ Sci & Technol, Future IT Innovat Lab, Pohang 790784, South Korea.
[Lee, Junyoung; Lee, Jeong-Soo] Pohang Univ Sci & Technol, Dept Elect Engn, Pohang 790784, South Korea.
[Meyyappan, Meyya] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
RP Kim, J (reprint author), Pohang Univ Sci & Technol, Div IT Convergence Engn, Pohang 790784, South Korea.
EM irijeori@postech.ac.kr; hacle@postech.ac.kr; covel123@postech.ac.kr;
baekck@postech.ac.kr; m.meyyappan@nasa.gov; ljs6951@postech.ac.kr
FU IT Consilience Creative Program [NIPA-2014-H0201-14-1001]; National IT
Industry Promotion Agency [2011-0031638]; Center for Advanced Soft
Electronics through the Ministry of Education, Science, and Technology,
Global Frontier Research Program, Korea; Pohang University of Science
and Technology, Pohang, Korea; Samsung Electronics Company, Ltd., Suwon,
Korea
FX This work was supported in part by the IT Consilience Creative Program
under Grant NIPA-2014-H0201-14-1001, in part by National IT Industry
Promotion Agency under Grant 2011-0031638, in part by Center for
Advanced Soft Electronics through the Ministry of Education, Science,
and Technology, Global Frontier Research Program, Korea, and in part by
the Semiconductor Industry Collaborative Project between Pohang
University of Science and Technology, Pohang, Korea, and Samsung
Electronics Company, Ltd., Suwon, Korea. The review of this paper was
arranged by Editor J. C. S. Woo.
NR 23
TC 3
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 0018-9383
EI 1557-9646
J9 IEEE T ELECTRON DEV
JI IEEE Trans. Electron Devices
PD AUG
PY 2014
VL 61
IS 8
BP 2705
EP 2710
DI 10.1109/TED.2014.2329848
PG 6
WC Engineering, Electrical & Electronic; Physics, Applied
SC Engineering; Physics
GA AQ6FS
UT WOS:000342906200014
ER
PT J
AU Pettorelli, N
Laurance, WF
O'Brien, TG
Wegmann, M
Nagendra, H
Turner, W
AF Pettorelli, Nathalie
Laurance, William F.
O'Brien, Timothy G.
Wegmann, Martin
Nagendra, Harini
Turner, Woody
TI Satellite remote sensing for applied ecologists: opportunities and
challenges
SO JOURNAL OF APPLIED ECOLOGY
LA English
DT Review
DE biodiversity; Earth observations; environmental management; natural
capital; sensor; technology; wildlife management
ID LAND-COVER CLASSIFICATIONS; PROTECTED AREAS; RAIN-FORESTS; INVASIVE
PLANT; BIODIVERSITY; RESOLUTION; IMAGERY; SPACE; RADAR; CONSERVATION
AB 1. Habitat loss and degradation, overexploitation, climate change and the spread of invasive species are drastically depleting the Earth's biological diversity, leading to detrimental impacts on ecosystem services and human well-being.
2. Our ability to monitor the state of biodiversity and the impacts of global environmental change on this natural capital is fundamental to designing effective adaptation and mitigation strategies for preventing further loss of biological diversity. This requires the scientific community to assess spatio-temporal changes in the distribution of abiotic conditions (e. g. temperature, rainfall) and in the distribution, structure, composition and functioning of ecosystems.
3. The potential for satellite remote sensing (SRS) to provide key data has been highlighted by many researchers, with SRS offering repeatable, standardized and verifiable information on long-term trends in biodiversity indicators. SRS permits one to address questions on scales inaccessible to ground-based methods alone, facilitating the development of an integrated approach to natural resource management, where biodiversity, pressures to biodiversity and consequences of management decisions can all be monitored.
4. Synthesis and applications. Here, we provide an interdisciplinary perspective on the prospects of satellite remote sensing (SRS) for ecological applications, reviewing established avenues and highlighting new research and technological developments that have a high potential to make a difference in environmental management. We also discuss current barriers to the ecological application of SRS-based approaches and identify possible ways to overcome some of these limitations.
C1 [Pettorelli, Nathalie] Zool Soc London, Inst Zool, London NW1 4RY, England.
[Laurance, William F.] James Cook Univ, Ctr Trop Environm & Sustainabil Sci, Cairns, Qld 4878, Australia.
[Laurance, William F.] James Cook Univ, Sch Marine & Trop Biol, Cairns, Qld 4878, Australia.
[O'Brien, Timothy G.] Wildlife Conservat Soc, Mpala Res Ctr, Nanyuki 10400, Kenya.
[Wegmann, Martin] Dept Geog & Geol, D-97074 Wurzburg, Germany.
[Nagendra, Harini] Azim Premji Univ, Bangalore 560100, Karnataka, India.
[Turner, Woody] NASA Headquarters, Div Earth Sci, Washington, DC 20546 USA.
RP Pettorelli, N (reprint author), Zool Soc London, Inst Zool, Regents Pk, London NW1 4RY, England.
EM nathalie.pettorelli@ioz.ac.uk
RI Research ID, CTBCC /O-3564-2014; James Cook University,
TESS/B-8171-2012;
OI Wegmann, Martin/0000-0003-0335-9601; Nagendra,
Harini/0000-0002-1585-0724
NR 112
TC 42
Z9 42
U1 22
U2 159
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 0021-8901
EI 1365-2664
J9 J APPL ECOL
JI J. Appl. Ecol.
PD AUG
PY 2014
VL 51
IS 4
BP 839
EP 848
DI 10.1111/1365-2664.12261
PG 10
WC Biodiversity Conservation; Ecology
SC Biodiversity & Conservation; Environmental Sciences & Ecology
GA AQ5LP
UT WOS:000342851000002
ER
PT J
AU Khazanov, G
Sibeck, D
Tel'nikhin, A
Kronberg, T
AF Khazanov, G.
Sibeck, D.
Tel'nikhin, A.
Kronberg, T.
TI Relativistic electron precipitation events driven by electromagnetic
ion-cyclotron waves
SO PHYSICS OF PLASMAS
LA English
DT Article
ID EMIC WAVES; MAGNETOSPHERE; LOSSES; PLASMA; STORMS
AB We adopt a canonical approach to describe the stochastic motion of relativistic belt electrons and their scattering into the loss cone by nonlinear EMIC waves. The estimated rate of scattering is sufficient to account for the rate and intensity of bursty electron precipitation. This interaction is shown to result in particle scattering into the loss cone, forming similar to 10 s microbursts of precipitating electrons. These dynamics can account for the statistical correlations between processes of energization, pitch angle scattering, and relativistic electron precipitation events, that are manifested on large temporal scales of the order of the diffusion time similar to tens of minutes. (C) 2014 AIP Publishing LLC.
C1 [Khazanov, G.; Sibeck, D.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Tel'nikhin, A.; Kronberg, T.] Altai State Univ, Dept Phys & Technol, Barnaul 656099, Russia.
RP Khazanov, G (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
EM george.v.khazanov@nasa.gov
RI feggans, john/F-5370-2012
FU NASA Van Allen Probes; NASA LWS Program; Altai State University (Russian
Federation)
FX Funding support for this study was provided by NASA Van Allen Probes
(formerly known as the Radiation Belt Storm Probes (RBSP)) Project, the
NASA LWS Program, and Altai State University (Russian Federation).
NR 27
TC 1
Z9 1
U1 0
U2 9
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
EI 1089-7674
J9 PHYS PLASMAS
JI Phys. Plasmas
PD AUG
PY 2014
VL 21
IS 8
AR 082901
DI 10.1063/1.4892185
PG 8
WC Physics, Fluids & Plasmas
SC Physics
GA AQ4IZ
UT WOS:000342760600056
ER
PT J
AU Mackey, J
Dynys, F
Sehirlioglu, A
AF Mackey, Jon
Dynys, Frederick
Sehirlioglu, Alp
TI Uncertainty analysis for common Seebeck and electrical resistivity
measurement systems
SO REVIEW OF SCIENTIFIC INSTRUMENTS
LA English
DT Article
ID THERMAL-CONDUCTIVITY; HIGH-TEMPERATURE; THERMOELECTRIC PROPERTIES;
COEFFICIENT; THERMOPOWER; APPARATUS; POWER
AB This work establishes the level of uncertainty for electrical measurements commonly made on thermoelectric samples. The analysis targets measurement systems based on the four probe method. Sources of uncertainty for both electrical resistivity and Seebeck coefficient were identified and evaluated. Included are reasonable estimates on the magnitude of each source, and cumulative propagation of error. Uncertainty for the Seebeck coefficient includes the cold-finger effect which has been quantified with thermal finite element analysis. The cold-finger effect, which is a result of parasitic heat transfer down the thermocouple probes, leads to an asymmetric over-estimation of the Seebeck coefficient. A silicon germanium thermoelectric sample has been characterized to provide an understanding of the total measurement uncertainty. The electrical resistivity was determined to contain uncertainty of +/- 7.0% across any measurement temperature. The Seebeck coefficient of the system is +1.0%/-13.1% at high temperature and +/- 1.0% near room temperature. The power factor has a combined uncertainty of +7.3%/-27.0% at high temperature and +/- 7.5% near room temperature. These ranges are calculated to be typical values for a general four probe Seebeck and resistivity measurement configuration. (C) 2014 AIP Publishing LLC.
C1 [Mackey, Jon] Univ Akron, Dept Mech Engn, Akron, OH 44325 USA.
[Dynys, Frederick] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA.
[Sehirlioglu, Alp] Case Western Reserve Univ, Dept Mat Sci & Engn, Cleveland, OH 44106 USA.
RP Mackey, J (reprint author), Univ Akron, Dept Mech Engn, Akron, OH 44325 USA.
EM jam151@zips.uakron.edu
FU NASA/USRA [04555-004]
FX The authors of this work would like to thank the assistance of Tom Sabo,
Ben Kowalski, and Ray Babuder from NASA Glenn Research Center (GRC), and
funding provided by NASA/USRA Contract No. 04555-004.
NR 33
TC 16
Z9 16
U1 3
U2 26
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
EI 1089-7623
J9 REV SCI INSTRUM
JI Rev. Sci. Instrum.
PD AUG
PY 2014
VL 85
IS 8
AR 085119
DI 10.1063/1.4893652
PG 10
WC Instruments & Instrumentation; Physics, Applied
SC Instruments & Instrumentation; Physics
GA AQ6IH
UT WOS:000342913500086
PM 25173324
ER
PT J
AU Hossain, F
Siddique-E-Akbor, AHM
Yigzaw, W
Shah-Newaz, S
Hossain, M
Mazumder, LC
Ahmed, T
Shum, CK
Lee, H
Biancamaria, S
Turk, FJ
Limaye, A
AF Hossain, Faisal
Siddique-E-Akbor, A. H. M.
Yigzaw, Wondmagegn
Shah-Newaz, Sardar
Hossain, Monowar
Mazumder, Liton Chandra
Ahmed, Tanvir
Shum, C. K.
Lee, Hyongki
Biancamaria, Sylvain
Turk, Francis J.
Limaye, Ashutosh
TI CROSSING THE "VALLEY OF DEATH" Lessons Learned from Implementing an
Operational Satellite-Based Flood Forecasting System
SO BULLETIN OF THE AMERICAN METEOROLOGICAL SOCIETY
LA English
DT Article
C1 [Hossain, Faisal; Siddique-E-Akbor, A. H. M.; Yigzaw, Wondmagegn] Tennessee Technol Univ, Dept Civil & Environm Engn, Cookeville, TN 38505 USA.
[Shah-Newaz, Sardar; Hossain, Monowar; Mazumder, Liton Chandra; Ahmed, Tanvir] Inst Water Modelling, Dhaka, Bangladesh.
[Shum, C. K.] Ohio State Univ, Columbus, OH 43210 USA.
[Shum, C. K.] Chinese Acad Sci, Inst Geodesy & Geophys, Beijing, Peoples R China.
[Lee, Hyongki] Univ Houston, Houston, TX USA.
[Biancamaria, Sylvain] CNRS, Lab Etud Geophys & Oceanog Spatiales, Toulouse, France.
[Turk, Francis J.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Limaye, Ashutosh] NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA.
RP Hossain, F (reprint author), Univ Washington, 201 More Hall,Box 352700, Seattle, WA 98105 USA.
EM fhossain@uw.edu
NR 12
TC 6
Z9 6
U1 1
U2 6
PU AMER METEOROLOGICAL SOC
PI BOSTON
PA 45 BEACON ST, BOSTON, MA 02108-3693 USA
SN 0003-0007
EI 1520-0477
J9 B AM METEOROL SOC
JI Bull. Amer. Meteorol. Soc.
PD AUG
PY 2014
VL 95
IS 8
BP 1201
EP 1207
DI 10.1175/BAMS-D-13-00176.1
PG 7
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA AQ1PD
UT WOS:000342552400008
ER
PT J
AU Vinogradova, NT
Ponte, RM
Fukumori, I
Wang, O
AF Vinogradova, Nadya T.
Ponte, Rui M.
Fukumori, Ichiro
Wang, Ou
TI Estimating satellite salinity errors for assimilation of Aquarius and
SMOS data into climate models
SO JOURNAL OF GEOPHYSICAL RESEARCH-OCEANS
LA English
DT Article
ID SEA-SURFACE SALINITY; OCEAN; CIRCULATION; PERFORMANCE
AB Constraining dynamical systems with new information from ocean measurements, including observations of sea surface salinity (SSS) from Aquarius and SMOS, requires careful consideration of data errors that are used to determine the importance of constraints in the optimization. Here such errors are derived by comparing satellite SSS observations from Aquarius and SMOS with ocean model output and in situ data. The associated data error variance maps have a complex spatial pattern, ranging from less than 0.05 in the open ocean to 1-2 (units of salinity variance) along the coasts and high latitude regions. Comparing the data-model misfits to the data errors indicates that the Aquarius and SMOS constraints could potentially affect estimated SSS values in several ocean regions, including most tropical latitudes. In reference to the Aquarius error budget, derived errors are less than the total allocation errors for the Aquarius mission accuracy requirements in low and midlatitudes, but exceed allocation errors in high latitudes.
C1 [Vinogradova, Nadya T.; Ponte, Rui M.] Atmospher & Environm Res Inc AER, Lexington, MA 02421 USA.
[Fukumori, Ichiro; Wang, Ou] NASA, Jet Prop Lab, Pasadena, CA USA.
RP Vinogradova, NT (reprint author), Atmospher & Environm Res Inc AER, Lexington, MA 02421 USA.
EM nadya@aer.com
FU NASA's Physical Oceanography Program; Ocean Surface Salinity Project
[NNH10CC10C, NNH14CL48C]; Spanish National Program on Space
FX This work was supported by NASA's Physical Oceanography Program and the
Ocean Surface Salinity Project through contracts NNH10CC10C and
NNH14CL48C to AER. Aquarius data are provided by NASA's Physical
Oceanography Distributed Active Archive Center (PO.DAAC) and can be
accessed at: http://podaac.jpl.nasa.gov/SeaSurfaceSalinity/Aquarius.
SMOS data were produced by the Barcelona Expert Center
(www.smos-bec.icm.csic.es), a joint initiative of the Spanish Research
Council (CSIC) and the Technical University of Catalonia (UPC), mainly
funded by the Spanish National Program on Space. SMOS data access:
http://cp34-bec.cmima.csic.es/thredds/catalog/REPOI_001M025B/catalog.htm
l. The in situ data used in this paper are available at
http://www.metoffice.gov.uk/hadobs/en3/data/EN3_v2a/download_EN3_v2a.htm
l. We thank our ECCO colleagues from MIT, Gael Forget and Patrick
Heimbach, for all their efforts on the production of ECCO-version 4. We
appreciate useful feedback and suggestions from two anonymous reviewers
and the Associate Editor who helped us improve our manuscript.
NR 28
TC 7
Z9 7
U1 3
U2 15
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 AUG
PY 2014
VL 119
IS 8
BP 4732
EP 4744
DI 10.1002/2014JC009906
PG 13
WC Oceanography
SC Oceanography
GA AQ1CR
UT WOS:000342519500003
ER
PT J
AU Tang, WQ
Yueh, SH
Fore, AG
Hayashi, A
Lee, T
Lagerloef, G
AF Tang, Wenqing
Yueh, Simon H.
Fore, Alexander G.
Hayashi, Akiko
Lee, Tong
Lagerloef, Gary
TI Uncertainty of Aquarius sea surface salinity retrieved under rainy
conditions and its implication on the water cycle study
SO JOURNAL OF GEOPHYSICAL RESEARCH-OCEANS
LA English
DT Article
ID DIELECTRIC-CONSTANT; OCEAN ALGORITHM; MIXED-LAYER; ARGO; TEMPERATURE;
VARIABILITY; BACKSCATTER; CHALLENGE; MODEL
AB The uncertainty of Aquarius sea surface salinity (SSS) retrieved under rain is assessed. Rain not only has instantaneous impact on SSS but also interferes with the microwave remote sensing signals, making the task to retrieve SSS under rainy conditions difficult. A rain correction model is developed based on analysis of the L-band radiometer/scatterometer residual signals after accounting for roughness due to wind and flat surface emissivity. The combined active passive algorithm is used to retrieve SSS in parallel with (CAP_RC) or without rain correction (CAP). The CAP bias against individual ARGO floats increases with rain rate with slope of -0.14 PSU per mm h(-1), which reduced to near zero in CAP_RC. On the global monthly basis, CAP_RC is about 0.03 PSU higher than CAP. RMSD against ARGO is slightly smaller for CAP_RC than CAP. Regional biases are examined in areas with frequent rain events. As expected, results show that Delta SSS (CAP_RC-CAP) is highly correlated with the seasonal precipitation pattern, reaching about 0.2-0.3 PSU under heavy rain. However, Delta SSS shows no correlation with the difference pattern between ARGO and CAP or CAP_RC. This, along with regional analyses, suggests that the difference between ARGO and Aquarius' SSS is likely caused by the different spatial and temporal sampling, in addition to near surface stratification depicted by radiometer and ARGO at different depths. The effect of Delta SSS on water cycle in terms of mixed-layer salt storage tendency is about 10% in areas where evaporation-minus-precipitation is the dominant process driving the variability of near surface salinity.
C1 [Tang, Wenqing; Yueh, Simon H.; Fore, Alexander G.; Hayashi, Akiko; Lee, Tong] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
[Lagerloef, Gary] Earth & Space Res, Seattle, WA USA.
RP Tang, WQ (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
EM Wenqing.Tang@jpl.nasa.gov
FU National Aeronautics and Space Administration
FX The work described in this paper carried out by the Jet Propulsion
Laboratory, California Institute of Technology was under a contract with
the National Aeronautics and Space Administration. The authors thank two
anonymous reviewers for their comments for improving this article.
Aquarius SSS data are available from http://podaac.jpl.nasa.gov; SSMI/S
and WindSAT rain data are downloaded from www.remss.com; ARGO monthly
gridded data from http://www.jamstec.go.jp/ARGO; ARGO individual floats
data collocated with Aquarius from https://aquarius.esr.org/avds; and
OAFlux evaporation from http://oaflux.whoi.edu.
NR 32
TC 13
Z9 13
U1 1
U2 13
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 AUG
PY 2014
VL 119
IS 8
BP 4821
EP 4839
DI 10.1002/2014JC009834
PG 19
WC Oceanography
SC Oceanography
GA AQ1CR
UT WOS:000342519500008
ER
PT J
AU Martin, ACH
Boutin, J
Hauser, D
Dinnat, EP
AF Martin, A. C. H.
Boutin, J.
Hauser, D.
Dinnat, E. P.
TI Active-passive synergy for interpreting ocean L-band emissivity: Results
from the CAROLS airborne campaigns
SO JOURNAL OF GEOPHYSICAL RESEARCH-OCEANS
LA English
DT Article
ID SEA-SURFACE SALINITY; MICROWAVE RADIOMETRY; FIELD EXPERIMENTS; SMOS;
RFI; MODEL
AB The impact of the ocean surface roughness on the ocean L-band emissivity is investigated using simultaneous airborne measurements from an L-band radiometer (CAROLS) and from a C-band scatterometer (STORM) acquired in the Gulf of Biscay (off-the French Atlantic coasts) in November 2010. Two synergetic approaches are used to investigate the impact of surface roughness on the L-band brightness temperature (Tb). First, wind derived from the scatterometer measurements is used to analyze the roughness contribution to Tb as a function of wind and compare it with the one simulated by SMOS and Aquarius roughness models. Then residuals from this mean relationship are analyzed in terms of mean square slope derived from the STORM instrument. We show improvement of new radiometric roughness models derived from SMOS and Aquarius satellite measurements in comparison with prelaunch models. Influence of wind azimuth on Tb could not be evidenced from our data set. However, we point out the importance of taking into account large roughness scales (>20 cm) in addition to small roughness scale (5 cm) rapidly affected by wind to interpret radiometric measurements far from nadir. This was made possible thanks to simultaneous estimates of large and small roughness scales using STORM at small (7-16 degrees) and large (30 degrees) incidence angles.
C1 [Martin, A. C. H.; Boutin, J.] Univ Paris 06, Sorbonne Univ, IRD, MNHN,LOCEAN IPSL, Paris, France.
[Martin, A. C. H.] Natl Oceanog Ctr, Southampton, Hants, England.
[Hauser, D.] Univ Paris 06, Sorbonne Univ, Univ Versailles St Quentin, CNRS,LATMOS IPSL, Guyancourt, France.
[Dinnat, E. P.] Chapman Univ, Ctr Excellence Earth Syst Modeling & Observat, Orange, CA USA.
[Dinnat, E. P.] NASA, Goddard Space Flight Ctr, Cryospher Sci Lab, Greenbelt, MD 20771 USA.
RP Martin, ACH (reprint author), Univ Paris 06, Sorbonne Univ, IRD, MNHN,LOCEAN IPSL, Paris, France.
EM admartin@noc.ac.uk
RI Dinnat, Emmanuel/D-7064-2012; Boutin, Jacqueline/M-2253-2016
OI Dinnat, Emmanuel/0000-0001-9003-1182;
FU French Space Agency CNES/TOSCA; CNES/CNRS grant
FX The authors acknowledge Mehrez Zribi, Pascal Fanise, and Mickael Parde
for providing CAROLS measurements. The authors wish to thank the crew of
the RV Cotes de la Manche as well as the technical teams from SAFIRE and
DT-INSU. The authors also thank Gerard Caudal and Xiaobin Yin for very
fruitful discussions, Joe Tenerelli for providing the Terrestrial
Radiometry Analysis Package and Nicolas Martin for computation support.
The authors thank Meteo France for providing data for the Gascogne Buoy
and for providing us support during the airborne campaign. The authors
also acknowledge Remote Sensing Systems for providing free and open
access to SSMIS measurements. The development of the CAROLS instrument
and the flight campaigns have been funded through the support of the
French Space Agency CNES/TOSCA. Adrien Martin has been funded by a
CNES/CNRS grant.
NR 47
TC 2
Z9 2
U1 0
U2 4
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 AUG
PY 2014
VL 119
IS 8
BP 4940
EP 4957
DI 10.1002/2014JC009890
PG 18
WC Oceanography
SC Oceanography
GA AQ1CR
UT WOS:000342519500013
ER
PT J
AU Yueh, S
Tang, WQ
Fore, A
Hayashi, A
Song, YT
Lagerloef, G
AF Yueh, Simon
Tang, Wenqing
Fore, Alexander
Hayashi, Akiko
Song, Yuhe T.
Lagerloef, Gary
TI Aquarius geophysical model function and combined active passive
algorithm for ocean surface salinity and wind retrieval
SO JOURNAL OF GEOPHYSICAL RESEARCH-OCEANS
LA English
DT Article
ID SEA-SURFACE; DIELECTRIC-CONSTANT; TEMPERATURE; CHALLENGE; WATER; ARGO
AB This paper describes the updated Combined Active-Passive (CAP) retrieval algorithm for simultaneous retrieval of surface salinity and wind from Aquarius' brightness temperature and radar backscatter. Unlike the algorithm developed by Remote Sensing Systems (RSS), implemented in the Aquarius Data Processing System (ADPS) to produce Aquarius standard products, the Jet Propulsion Laboratory's CAP algorithm does not require monthly climatology SSS maps for the salinity retrieval. Furthermore, the ADPS-RSS algorithm fully uses the National Center for Environmental Predictions (NCEP) wind for data correction, while the CAP algorithm uses the NCEP wind only as a constraint. The major updates to the CAP algorithm include the galactic reflection correction, Faraday rotation, Antenna Pattern Correction, and geophysical model functions of wind or wave impacts. Recognizing the limitation of geometric optics scattering, we improve the modeling of the reflection of galactic radiation; the results are better salinity accuracy and significantly reduced ascending-descending bias. We assess the accuracy of CAP's salinity by comparison with ARGO monthly gridded salinity products provided by the Asia-Pacific Data-Research Center (APDRC) and Japan Agency for Marine-Earth Science and Technology (JAMSTEC). The RMS differences between Aquarius CAP and APDRC's or JAMSTEC's ARGO salinities are less than 0.2 psu for most parts of the ocean, except for the regions in the Intertropical Convergence Zone, near the outflow of major rivers and at high latitudes.
C1 [Yueh, Simon; Tang, Wenqing; Fore, Alexander; Hayashi, Akiko; Song, Yuhe T.; Lagerloef, Gary] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
RP Yueh, S (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
EM Simon.Yueh@jpl.nasa.gov
FU National Aeronautics and Space Administration
FX The work described in this paper was carried out by the Jet Propulsion
Laboratory, California Institute of Technology under a contract with the
National Aeronautics and Space Administration. The Aquarius data were
obtained from the NASA Physical Oceanography Distributed Active Archive
Center, http://podaac.jpl.nasa.gov/aquarius.
NR 38
TC 16
Z9 16
U1 1
U2 11
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 AUG
PY 2014
VL 119
IS 8
BP 5360
EP 5379
DI 10.1002/2014JC009939
PG 20
WC Oceanography
SC Oceanography
GA AQ1CR
UT WOS:000342519500037
ER
PT J
AU Webster, MA
Rigor, IG
Nghiem, SV
Kurtz, NT
Farrell, SL
Perovich, DK
Sturm, M
AF Webster, Melinda A.
Rigor, Ignatius G.
Nghiem, Son V.
Kurtz, Nathan T.
Farrell, Sinead L.
Perovich, Donald K.
Sturm, Matthew
TI Interdecadal changes in snow depth on Arctic sea ice
SO JOURNAL OF GEOPHYSICAL RESEARCH-OCEANS
LA English
DT Article
ID THERMAL-CONDUCTIVITY; THICKNESS; PRODUCTS
AB Snow plays a key role in the growth and decay of Arctic sea ice. In winter, it insulates sea ice from cold air temperatures, slowing sea ice growth. From spring to summer, the albedo of snow determines how much insolation is absorbed by the sea ice and underlying ocean, impacting ice melt processes. Knowledge of the contemporary snow depth distribution is essential for estimating sea ice thickness and volume, and for understanding and modeling sea ice thermodynamics in the changing Arctic. This study assesses spring snow depth distribution on Arctic sea ice using airborne radar observations from Operation IceBridge for 2009-2013. Data were validated using coordinated in situ measurements taken in March 2012 during the Bromine, Ozone, and Mercury Experiment (BROMEX) field campaign. We find a correlation of 0.59 and root-mean-square error of 5.8 cm between the airborne and in situ data. Using this relationship and Ice-Bridge snow thickness products, we compared the recent results with data from the 1937, 1954-1991 Soviet drifting ice stations. The comparison shows thinning of the snowpack, from 35.1 +/- 9.4 to 22.2 +/- 1.9 cm in the western Arctic, and from 32.8 +/- 9.4 to 14.5 +/- 1.9 cm in the Beaufort and Chukchi seas. These changes suggest a snow depth decline of 37 +/- 29% in the western Arctic and 56 +/- 33% in the Beaufort and Chukchi seas. Thinning is negatively correlated with the delayed onset of sea ice freezeup during autumn.
C1 [Webster, Melinda A.; Rigor, Ignatius G.] Univ Washington, Appl Phys Lab, Polar Sci Ctr, Seattle, WA 98105 USA.
[Nghiem, Son V.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Kurtz, Nathan T.; Farrell, Sinead L.] NASA, Goddard Space Flight Ctr, Hydrospher & Biospher Sci Lab, Greenbelt, MD 20771 USA.
[Farrell, Sinead L.] Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20742 USA.
[Perovich, Donald K.] US Army Corps Engineers, Engn Res & Dev Ctr, Cold Reg Res & Engn Lab, Hanover, NH USA.
[Sturm, Matthew] Univ Alaska Fairbanks, Inst Geophys, Fairbanks, AK 99775 USA.
RP Webster, MA (reprint author), Univ Washington, Appl Phys Lab, Polar Sci Ctr, Seattle, WA 98105 USA.
EM melindaw@uw.edu
RI Farrell, Sinead/F-5586-2010
OI Farrell, Sinead/0000-0003-3222-2751
FU NASA Cryospheric Sciences Program
FX Snow data from the 2012 BROMEX field campaign are available upon
request. Meteorological data are available at
http://www.esrl.noaa.gov/gmd/dv/. The IceBridge quick-look and standard
snow depth products are available at https://nsidc.org/data/docs
/daac/icebridge/evaluation_products/sea-ice-freeboard-snowdepththickness
-quicklook-index.html and http://nsidc. org/data/idcsi2.html. The Soviet
station snow data are available at http://dx.doi.org/10.7265/N5MS3QNJ.
Ice Mass Balance buoy data are available at
http://IMB.crrel.usace.army.mil. The sea ice freezeup product from
passive microwave satellite data is available at
http://neptune.gsfc.nasa.gov/csb/index.php? section=54. This research
was supported by the National Aeronautics and Space Administration
(NASA), and by contributors to the U.S. Interagency Arctic Buoy Program,
which include the U.S. Coast Guard, NAVO, NIC, NOAA, NSF, and ONR. This
is JISAO contribution 2225. The research carried out at the Jet
Propulsion Laboratory, California Institute of Technology, was supported
by the NASA Cryospheric Sciences Program. We thank Jacqueline A.
Richter-Menge of the U.S. Army Cold Regions Research and Engineering
Laboratory for the planning and coordination of the IceBridge flight
operation with the BROMEX field campaign, and Stephen Warren for helpful
discussions. We thank UMIAQ, the Barrow whaling community, and the
Barrow Arctic Science Consortium for their assistance in the BROMEX
field campaign.
NR 42
TC 27
Z9 28
U1 4
U2 29
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 AUG
PY 2014
VL 119
IS 8
BP 5395
EP 5406
DI 10.1002/2014JC009985
PG 12
WC Oceanography
SC Oceanography
GA AQ1CR
UT WOS:000342519500039
ER
PT J
AU Chaussard, E
Burgmann, R
Shirzaei, M
Fielding, EJ
Baker, B
AF Chaussard, E.
Buergmann, R.
Shirzaei, M.
Fielding, E. J.
Baker, B.
TI Predictability of hydraulic head changes and characterization of
aquifer-system and fault properties from InSAR-derived ground
deformation
SO JOURNAL OF GEOPHYSICAL RESEARCH-SOLID EARTH
LA English
DT Article
ID APERTURE RADAR INTERFEROMETRY; SANTA-CLARA-VALLEY; LAS-VEGAS VALLEY;
LAND SUBSIDENCE; PRINCIPAL COMPONENTS; SURFACE DEFORMATION; HAYWARD
FAULT; CALIFORNIA; BASIN; SAR
AB We evaluate the benefits of space-derived ground deformation measurements for basin-wide characterization of aquifer-system properties and groundwater levels. We use Interferometric Synthetic Aperture Radar (InSAR) time series analysis of ERS, Envisat, and ALOS SAR data to resolve 1992-2011 ground deformation in the Santa Clara Valley, California. T-mode principal component analysis successfully isolates temporally variable deformation patterns embedded in the multidecadal time series. The data reveal uplift at 0.4 cm/yr between 1992 and 2000 and <0.1 cm/yr during 2000-2011, illustrating the end of the aquifer-system's poroelastic rebound following recovery of hydraulic heads after the 1960s low stand. In addition, seasonal elastic deformation with amplitude of up to 3 cm, in phase with head fluctuations, is observed over the confined aquifer sharply partitioned by the Quaternary Silver Creek Fault (SCF). Integration of this deformation with hydraulic head data enables characterization of the aquifer-system storativity and elastic skeletal specific storage. Modeling of the deformation partitioning across the SCF constrains the fault's last tectonic activity, hydraulic conductivity, and material composition. The SCF likely cuts the shallow confining clays and was last active since similar to 140 ka, it has a horizontal hydraulic conductivity several orders of magnitude lower than the surrounding aquifer-system, and is likely composed of clays, making it an effective barrier to across-fault fluid flow. Finally, we show that after a period of calibration, InSAR can be used to characterize basin-wide water level changes without well measurements with an accuracy of 70%, which demonstrates that it provides useful data for groundwater management.
C1 [Chaussard, E.; Buergmann, R.] Univ Calif Berkeley, Dept Earth & Planetary Sci, Berkeley, CA 94720 USA.
[Chaussard, E.; Buergmann, R.] Univ Calif Berkeley, Berkeley Seismol Lab, Berkeley, CA 94720 USA.
[Shirzaei, M.] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ USA.
[Fielding, E. J.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Baker, B.] Santa Clara Valley Water Dist, San Jose, CA USA.
RP Chaussard, E (reprint author), Univ Calif Berkeley, Dept Earth & Planetary Sci, Berkeley, CA 94720 USA.
EM estelle@seismo.berkeley.edu
OI Chaussard, Estelle/0000-0002-2291-7085
FU National Aeronautics and Space Administration (NASA) [NNX12AQ32G]; Earth
Surface and Interior focus area at NASA
FX We thank the National Aeronautics and Space Administration (NASA) for
support through grant NNX12AQ32G. We thank Thomas Burbey and Devin
Galloway for their thoughtful comments prior to submission. We also
thank the Associate Editor, Devin Galloway, and an anonymous reviewer
for the reviews, which helped improve the quality of the manuscript. We
thank the Santa Clara Valley Water District for the hydraulic head data.
The ERS and Envisat original data are copyrighted by the European Space
Agency and were provided through the WInSAR archive. The ALOS-PALSAR
data are copyrighted by the Japanese Aerospace Exploration Agency (JAXA)
and Ministry of Economy, Trade, and Industry and were made available by
the U.S. Government Research Consortium through the Alaska Satellite
Facility. Part of this research was supported by the Earth Surface and
Interior focus area at NASA and performed at the Jet Propulsion
Laboratory, California Institute of Technology.
NR 94
TC 20
Z9 20
U1 3
U2 25
PU AMER GEOPHYSICAL UNION
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 AUG
PY 2014
VL 119
IS 8
BP 6572
EP 6590
DI 10.1002/2014JB011266
PG 19
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA AQ1AD
UT WOS:000342512900025
ER
PT J
AU Force, DA
AF Force, Dale A.
TI Shaped, Fixed Antenna for One Gigabit per Second Data Rate Transmission
from Earth Exploration Satellites in Low Earth Orbit
SO IEEE AEROSPACE AND ELECTRONIC SYSTEMS MAGAZINE
LA English
DT Article
C1 [Force, Dale A.] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA.
RP Force, DA (reprint author), NASA, Glenn Res Ctr, Commun & Intelligent Syst Div, 21000 Brookpk Rd,MS 54-1, Cleveland, OH 44135 USA.
EM Dale.A.Force@nasa.gov
NR 10
TC 0
Z9 0
U1 0
U2 1
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 0885-8985
EI 1557-959X
J9 IEEE AERO EL SYS MAG
JI IEEE Aerosp. Electron. Syst. Mag.
PD AUG
PY 2014
VL 29
IS 8
BP 4
EP 9
DI 10.1109/MAES.2014.120067
PG 6
WC Engineering, Aerospace; Engineering, Electrical & Electronic
SC Engineering
GA AP7SZ
UT WOS:000342278300002
ER
PT J
AU Solomonidou, A
Hirtzig, M
Coustenis, A
Bratsolis, E
Le Mouelic, S
Rodriguez, S
Stephan, K
Drossart, P
Sotin, C
Jaumann, R
Brown, RH
Kyriakopoulos, K
Lopes, RMC
Bampasidis, G
Stamatelopoulou-Seymour, K
Moussas, X
AF Solomonidou, A.
Hirtzig, M.
Coustenis, A.
Bratsolis, E.
Le Mouelic, S.
Rodriguez, S.
Stephan, K.
Drossart, P.
Sotin, C.
Jaumann, R.
Brown, R. H.
Kyriakopoulos, K.
Lopes, R. M. C.
Bampasidis, G.
Stamatelopoulou-Seymour, K.
Moussas, X.
TI Surface albedo spectral properties of geologically interesting areas on
Titan
SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS
LA English
DT Article
ID HUYGENS LANDING SITE; 5 MU-M; CASSINI VIMS; POSSIBLE ORIGIN; RADAR
MAPPER; ATMOSPHERE; FEATURES; METHANE; MODEL; CRYOVOLCANISM
AB We investigate the nature and possible formation processes of three areas on Titan's surface which have been suggested as geologically interesting: Hotei Regio, Tui Regio, and Sotra Patera. We also reanalyze the spectral characteristics of the Huygens Landing Site. We apply a statistical Principal Component Analysis (PCA) and a radiative transfer (RT) method on the Visual and Infrared Mapping Spectrometer Datacubes in order to retrieve the surface albedo of distinct spectral units in the near infrared. We have been able to exploit only a subset of the currently available Hotei Regio data, which are, in general, not optimal in terms of geometry for an analysis with a plane-parallel RT code. Our inferred surface albedos present generally higher values from 1 to 2 mu m and lower ones at 0.94 and in the 2.6-5 mu m region. The Regions of Interest (RoIs) within Hotei Regio, Tui Regio, and Sotra Patera are always significantly brighter than the surrounding areas. The largest variations are found longward of 2 mu m and mainly at 5 mu m. This higher surface albedo with respect to the surrounding area and, in general, the fact that the spectral behavior is different for each of these areas, is probably indicative of diverse chemical compositions and origins. We compare the spectral albedos with some suggested surface candidates on Titan (such as H2O, CO2, and CH4 ices, as well as tholin) and discuss possible chemical composition variations as well as other interpretations.
C1 [Solomonidou, A.; Sotin, C.; Lopes, R. M. C.] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
[Solomonidou, A.; Hirtzig, M.; Coustenis, A.; Drossart, P.; Bampasidis, G.] Paris VI Paris Diderot Univ, UPMC Univ, CNRS, LESIA,Observ Paris, Meudon, France.
[Hirtzig, M.] Fdn Main Pate, Montrouge, France.
[Bratsolis, E.; Bampasidis, G.; Moussas, X.] Univ Athens, Dept Phys, Athens, Greece.
[Le Mouelic, S.] Univ Nantes, CNRS, UMR 6112, Lab Planetol & Geodynam,LPGNantes, Nantes, France.
[Rodriguez, S.] Univ Paris 07, CNRS, CEA Saclay, Lab AIM,DSM,IRFU,SAp, Paris, France.
[Stephan, K.; Jaumann, R.] DLR, Inst Planetary Res, Berlin, Germany.
[Brown, R. H.] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA.
[Kyriakopoulos, K.] Univ Athens, Dept Geol & Geoenvironm, Athens, Greece.
[Stamatelopoulou-Seymour, K.] Univ Patras, Dept Geol, Patras, Greece.
[Stamatelopoulou-Seymour, K.] Concordia Univ, Dept Geog, Montreal, PQ, Canada.
RP Solomonidou, A (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
EM Anezina.Solomonidou@jpl.nasa.gov
RI Lopes, Rosaly/D-1608-2016; Rodriguez, Sebastien/H-5902-2016
OI Lopes, Rosaly/0000-0002-7928-3167; Rodriguez,
Sebastien/0000-0003-1219-0641
FU European Union (European Social Fund-ESF); Operational Program
"Education and Lifelong Learning" of the National Strategic Reference
Framework (NSRF)-Research Funding Program: Heracleitus II; NASA; French
"Agence Nationale de la Recherche", France [11BS56002]
FX This research has been cofinanced by the European Union (European Social
Fund-ESF) and Greek national funds through the Operational Program
"Education and Lifelong Learning" of the National Strategic Reference
Framework (NSRF)-Research Funding Program: Heracleitus II. Investing in
knowledge society through the European Social Fund. The research was
also partly supported by an appointment to the NASA Postdoctoral Program
at the Jet Propulsion Laboratory, California Institute of Technology,
administered by Oak Ridge Associated Universities through a contract
with NASA. A. C., S. L. M., S. R., C. S., P. D., and M. H. acknowledge
financial support from the French "Agence Nationale de la Recherche"
(ANR Project: CH4@Titan and/or ANR project "APOSTIC" 11BS56002), France.
Part of the research was carried out by A. S. at the National and
Kapodistrian University of Athens, Department of Geology and
Geoenvironment. We thank Jason W. Barnes and an anonymous referee for
their thorough and constructive reviews of the manuscript.
NR 85
TC 11
Z9 11
U1 3
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 AUG
PY 2014
VL 119
IS 8
BP 1729
EP 1747
DI 10.1002/2014JE004634
PG 19
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA AQ0ZA
UT WOS:000342510000001
ER
PT J
AU Heavens, NG
Johnson, MS
Abdou, WA
Kass, DM
Kleinbohl, A
McCleese, DJ
Shirley, JH
Wilson, RJ
AF Heavens, Nicholas G.
Johnson, Morgan S.
Abdou, Wedad A.
Kass, David M.
Kleinboehl, Armin
McCleese, Daniel J.
Shirley, James H.
Wilson, R. John
TI Seasonal and diurnal variability of detached dust layers in the tropical
Martian atmosphere
SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS
LA English
DT Article
ID GENERAL-CIRCULATION MODEL; ORBITER CAMERA OBSERVATIONS; WATER-ICE
CLOUDS; MARS; CRYSTALS; AGGREGATION; SIMULATION; STORMS; CYCLE;
OCCULTATIONS
AB Evidence for widespread nonuniform vertical mixing of dust in Mars's tropical atmosphere (in the form of features called "detached dust layers" or DDLs) is a challenge for atmospheric modeling. We characterize the seasonal, diurnal, and geographic variability of DDL activity in retrievals from observations by the Mars Climate Sounder onboard Mars Reconnaissance Orbiter. We find that dust injection above the boundary layer, which forms DDLs, is a spatially ubiquitous phenomenon in the tropics during the daytime, implying that it has a significant nontopographic component. DDL formation is more intense in northern spring and summer than in southern spring and summer but is still common when the zonal average dust distribution appears uniformly mixed. DDLs do not appear to follow the upwelling associated with Mars's Hadley circulation or the extant climatology of local dust storm activity in the tropics. Geographic variability in the nightside vertical dust distribution does not always correlate with the dayside vertical dust distribution, implying that there is spatial and seasonal variability in the efficiency of dust deposition/removal processes. Nighttime dust removal is especially efficient over the Tharsis Montes during northern spring and summer, which suggests some association between water ice clouds and removal. Intense injection combined with efficient removal results in a high amplitude of diurnal variability in the dust distribution at 15-30 km above the surface of the tropics during much of the Martian year.
C1 [Heavens, Nicholas G.] Hampton Univ, Dept Atmospher & Planetary Sci, Hampton, VA 23668 USA.
[Johnson, Morgan S.] Rochester Inst Technol, Sch Phys & Astron, Rochester, NY 14623 USA.
[Abdou, Wedad A.; Kass, David M.; Kleinboehl, Armin; McCleese, Daniel J.; Shirley, James H.] CALTECH, Jet Prop Lab, NASA, Pasadena, CA USA.
[Wilson, R. John] NOAA, Geophys Fluid Dynam Lab, Princeton, NJ USA.
RP Heavens, NG (reprint author), Hampton Univ, Dept Atmospher & Planetary Sci, Hampton, VA 23668 USA.
EM nicholas.heavens@hamptonu.edu
OI Heavens, Nicholas/0000-0001-7654-503X
FU NASA Jet Propulsion Laboratory, California Institute of Technology
[1471216]
FX N.G. Heavens and M. S. Johnson acknowledge support from the NASA Jet
Propulsion Laboratory, California Institute of Technology (subcontract
1471216). M. S. Johnson was hosted at Hampton University as part of the
CREST Undergraduate Research Experience program. We thank Aymeric Spiga
and an anonymous reviewer for their thorough reviews, which
significantly improved this paper. All MRO-MCS data used to produce the
results of this paper are freely available from NASA's Planetary Data
System. Any analytical code is available from the first author by
request. NOAA GFDL Mars model output is available from author Wilson by
request.
NR 56
TC 5
Z9 5
U1 1
U2 13
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 AUG
PY 2014
VL 119
IS 8
BP 1748
EP 1774
DI 10.1002/2014JE004619
PG 27
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA AQ0ZA
UT WOS:000342510000002
ER
PT J
AU Jordan, AP
Stubbs, TJ
Wilson, JK
Schwadron, NA
Spence, HE
Joyce, CJ
AF Jordan, A. P.
Stubbs, T. J.
Wilson, J. K.
Schwadron, N. A.
Spence, H. E.
Joyce, C. J.
TI Deep dielectric charging of regolith within the Moon's permanently
shadowed regions
SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS
LA English
DT Article
ID LUNAR PLASMA WAKE; SOLID DIELECTRICS; SPACECRAFT; BREAKDOWN; PROTON;
ACCELERATION; ENVIRONMENT; FIELDS; PULSES; MODEL
AB Energetic charged particles, such as galactic cosmic rays (GCRs) and solar energetic particles (SEPs), can penetrate deep within the lunar surface, resulting in deep dielectric charging. This charging process depends on the GCR and SEP currents, as well as on the regolith's electrical conductivity and permittivity. In permanently shadowed regions (PSRs) near the lunar poles, the discharging timescales are on the order of a lunation (similar to 20 days). We present the first predictions for deep dielectric charging of lunar regolith. To estimate the resulting subsurface electric fields, we develop a data-driven, one-dimensional, time-dependent model. For model inputs, we use GCR data from the Cosmic Ray Telescope for the Effects of Radiation on board the Lunar Reconnaissance Orbiter and SEP data from the Electron, Proton, and Alpha Monitor on the Advanced Composition Explorer. We find that during the recent solar minimum, GCRs create persistent electric fields up to similar to 700 V/m. We also find that large SEP events create transient but strong electric fields (>= 10(6) V/m) that may induce dielectric breakdown. Such breakdown would likely result in significant modifications to the physical and chemical properties of the lunar regolith within PSRs.
C1 [Jordan, A. P.; Wilson, J. K.; Schwadron, N. A.; Spence, H. E.; Joyce, C. J.] Univ New Hampshire, Inst Study Earth Oceans & Space, Durham, NH 03824 USA.
[Stubbs, T. J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Jordan, AP (reprint author), Univ New Hampshire, Inst Study Earth Oceans & Space, Durham, NH 03824 USA.
EM a.p.jordan@unh.edu
RI Stubbs, Timothy/I-5139-2013
OI Stubbs, Timothy/0000-0002-5524-645X
FU NASA [NNG11PA03C, NNX10AB17A]
FX This work was supported by NASA grant NNG11PA03C and NNX10AB17A. The
authors wish to thank Larry Townsend for helpful discussions. The
authors also thank the ACE/EPAM team and its Principal Investigator
Robert Gold of JHU/APL for providing the ACE data via CDAWeb at
http://cdaweb.gsfc.nasa.gov/. LRO/CRaTER Level 2 data are available at
the NASA Planetary Data System at http://pds.nasa.gov. The PSTAR and
ESTAR results are available from the NIST website at
http://www.nist.gov.
NR 65
TC 5
Z9 5
U1 1
U2 4
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 AUG
PY 2014
VL 119
IS 8
BP 1806
EP 1821
DI 10.1002/2014JE004648
PG 16
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA AQ0ZA
UT WOS:000342510000004
ER
PT J
AU Martinez, GM
Renno, N
Fischer, E
Borlina, CS
Hallet, B
Juarez, MD
Vasavada, AR
Ramos, M
Hamilton, V
Gomez-Elvira, J
Haberle, RM
AF Martinez, G. M.
Renno, N.
Fischer, E.
Borlina, C. S.
Hallet, B.
Juarez, M. de la Torre
Vasavada, A. R.
Ramos, M.
Hamilton, V.
Gomez-Elvira, J.
Haberle, R. M.
TI Surface energy budget and thermal inertia at Gale Crater: Calculations
from ground-based measurements
SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS
LA English
DT Article
ID BOUNDARY-LAYER; EMISSION SPECTROMETER; TEMPERATURE SENSOR;
MERIDIANI-PLANUM; MARTIAN SURFACE; LANDING SITES; MARS; ROVER; MODEL;
WATER
AB The analysis of the surface energy budget (SEB) yields insights into soil-atmosphere interactions and local climates, while the analysis of the thermal inertia (I) of shallow subsurfaces provides context for evaluating geological features. Mars orbital data have been used to determine thermal inertias at horizontal scales of similar to 10(4) m(2) to similar to 10(7) m(2). Here we use measurements of ground temperature and atmospheric variables by Curiosity to calculate thermal inertias at Gale Crater at horizontal scales of similar to 10(2) m(2). We analyze three sols representing distinct environmental conditions and soil properties, sol 82 at Rocknest (RCK), sol 112 at Point Lake (PL), and sol 139 at Yellowknife Bay (YKB). Our results indicate that the largest thermal inertia I = 452 J m(-2) K-1 s(-1/2) (SI units used throughout this article) is found at YKB followed by PL with I = 306 and RCK with I = 295. These values are consistent with the expected thermal inertias for the types of terrain imaged by Mastcam and with previous satellite estimations at Gale Crater. We also calculate the SEB using data from measurements by Curiosity's Rover Environmental Monitoring Station and dust opacity values derived from measurements by Mastcam. The knowledge of the SEB and thermal inertia has the potential to enhance our understanding of the climate, the geology, and the habitability of Mars.
C1 [Martinez, G. M.; Renno, N.; Fischer, E.; Borlina, C. S.] Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA.
[Hallet, B.] Univ Washington, Dept Earth & Space Sci, Seattle, WA 98195 USA.
[Juarez, M. de la Torre; Vasavada, A. R.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Ramos, M.] Univ Alcala de Henares, Dept Fis, Madrid, Spain.
[Hamilton, V.] SW Res Inst, Dep Space Studies, Boulder, CO USA.
[Gomez-Elvira, J.] Ctr Astrobiol, Madrid, Spain.
[Haberle, R. M.] NASA, Ames Res Ctr, Div Space Sci, Moffett Field, CA 94035 USA.
RP Martinez, GM (reprint author), Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA.
EM gemartin@umich.edu
RI Ramos, Miguel/K-2230-2014
OI Ramos, Miguel/0000-0003-3648-6818
FU JPL [1449038]
FX This research is supported by a grant from JPL 1449038. German Martinez
wants to thank Harvey Elliott for his contribution to improve this work.
We want to thank Hanna Sizemore and the anonymous reviewer for their
excellent suggestions to improve the paper. We also thank the REMS Team
for their support of this investigation.
NR 42
TC 13
Z9 13
U1 0
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 AUG
PY 2014
VL 119
IS 8
BP 1822
EP 1838
DI 10.1002/2014JE004618
PG 17
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA AQ0ZA
UT WOS:000342510000005
ER
PT J
AU Arney, G
Meadows, V
Crisp, D
Schmidt, SJ
Bailey, J
Robinson, T
AF Arney, Giada
Meadows, Victoria
Crisp, David
Schmidt, Sarah J.
Bailey, Jeremy
Robinson, Tyler
TI Spatially resolved measurements of H2O, HCl, CO, OCS, SO2, cloud
opacity, and acid concentration in the Venus near-infrared spectral
windows
SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS
LA English
DT Article
ID LOWER ATMOSPHERE; DEEP ATMOSPHERE; WATER-VAPOR; DARK SIDE; RUNAWAY
GREENHOUSE; CARBON-MONOXIDE; NIGHT SIDE; LINE LIST; ABSORPTION;
SPECTROSCOPY
AB We observed Venus with the Apache Point Observatory 3.5 m telescope TripleSpec spectrograph (R = 3500, lambda = 0.96-2.47 mu m) on 1-3 March 2009 and on 25, 27, and 30 November and 2-4 December 2010. With these observations and synthetic spectra generated with the Spectral Mapping and Atmospheric Radiative Transfer model, we produce the first simultaneous maps of cloud opacity, acid concentration, water vapor (H2O), hydrogen chloride (HCl), carbon dioxide (CO), carbonyl sulfide (OCS), and sulfur dioxide (SO2) abundances in the Venusian lower atmosphere. Water measured at wavelengths near 1.18 mu m (near-surface) averages 29 +/- 2 ppm (2009) and 27 +/- 2 ppm (2010) and measured near 1.74 mu m (15-30 km) averages 33 +/- 2 ppm (2009) and 32 +/- 2 ppm (2010). Water in both these altitude ranges is spatially homogeneous. Water measured near 2.4 mu m (30-45 km) averages 34 +/- 2 ppm (2009) and 33 +/- 3 ppm (2010) and is spatially inhomogeneous and variable. HCl ismeasured near 1.74 mu m to be 0.41 +/- 0.04 ppm (2009) and 0.42 +/- 0.05 ppm (2010). CO and OCS (2.3-2.5 mu m; 30-45 km in altitude) are spatially inhomogeneous and show anticorrelation. CO (35 km) averages 25 +/- 3 ppm (2009) and 22 +/- 2 ppm (2010). OCS (36 km) averages 0.44 +/- 0.10 ppm (2009) and 0.57 +/- 0.12 ppm (2010). SO2 measurements average 140 +/- 37 ppm (2009) and 126 +/- 32 ppm (2010). Many species display a hemispherical dichotomy in their distribution. We find considerable spatial variability suggesting active processes with conservation between species. The most variable regions are just below the Venus cloud deck, and these may be related to changes in atmospheric circulation or virga events.
C1 [Arney, Giada; Meadows, Victoria] Univ Washington, Dept Astron, Seattle, WA 98195 USA.
[Arney, Giada; Meadows, Victoria] Univ Washington, Astrobiol Program, Seattle, WA 98195 USA.
[Arney, Giada; Meadows, Victoria; Crisp, David; Robinson, Tyler] NAI Virtual Planetary Lab, Seattle, WA USA.
[Crisp, David] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Schmidt, Sarah J.] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA.
[Bailey, Jeremy] Univ New S Wales, Sch Phys, Sydney, NSW, Australia.
[Robinson, Tyler] NASA Ames Explorat Ctr, Mountain View, CA USA.
RP Arney, G (reprint author), Univ Washington, Dept Astron, Seattle, WA 98195 USA.
EM giada@astro.washington.edu
FU National Aeronautics and Space Administration through NASA Astrobiology
Institute [NNH05ZDA001C, NNH12ZDA002C, NNA08CN87A, NNA13AA93A];
University of Washington eScience Institute
FX Observational data are available upon request from the author. This work
was performed as part of the NASA Astrobiology Institute's Virtual
Planetary Laboratory Lead Team, supported by the National Aeronautics
and Space Administration through the NASA Astrobiology Institute under
solicitations NNH05ZDA001C and NNH12ZDA002C and Cooperative Agreement
NNA08CN87A and NNA13AA93A. This work was additionally supported in part
by the University of Washington eScience Institute. We thank Y. Yung for
useful discussions and are grateful for our reviewers B. Bezard and
C.C.C. Tsang for their thoughtful comments and suggestions which helped
to improve the quality of this manuscript.
NR 81
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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 AUG
PY 2014
VL 119
IS 8
BP 1860
EP 1891
DI 10.1002/2014JE004662
PG 32
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA AQ0ZA
UT WOS:000342510000007
ER
PT J
AU Clifford, SM
Farmer, J
Carr, MH
Marais, DD
Bibring, JP
Craddock, R
Newsom, H
AF Clifford, Stephen M.
Farmer, Jack
Carr, Michael H.
Marais, Dave Des
Bibring, Jean-Pierre
Craddock, Robert
Newsom, Horton
TI Introduction to the Early Mars III Special Section and Key Questions
from the Third International Conference on Early Mars
SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS
LA English
DT Article
ID STRATIGRAPHY; EVENTS
C1 [Clifford, Stephen M.] Lunar & Planetary Inst, Houston, TX 77058 USA.
[Farmer, Jack] Arizona State Univ, Dept Geol, Tempe, AZ 85287 USA.
[Carr, Michael H.] US Geol Survey, Menlo Pk, CA 94025 USA.
[Marais, Dave Des] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Bibring, Jean-Pierre] IAS, Orsay, France.
[Craddock, Robert] Smithsonian Inst, Natl Air & Space Museum, Ctr Earth & Planetary Sci, Washington, DC 20560 USA.
[Newsom, Horton] Univ New Mexico, Inst Meteorit, Albuquerque, NM 87131 USA.
RP Clifford, SM (reprint author), Lunar & Planetary Inst, 3303 NASA Rd 1, Houston, TX 77058 USA.
EM clifford@lpi.usra.edu
NR 15
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U1 0
U2 5
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 AUG
PY 2014
VL 119
IS 8
BP 1892
EP 1894
DI 10.1002/2014JE004643
PG 3
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA AQ0ZA
UT WOS:000342510000008
ER
PT J
AU Zhang, G
Ganguly, S
Nemani, RR
White, MA
Milesi, C
Hashimoto, H
Wang, WL
Saatchi, S
Yu, YF
Myneni, RB
AF Zhang, Gong
Ganguly, Sangram
Nemani, Ramakrishna R.
White, Michael A.
Milesi, Cristina
Hashimoto, Hirofumi
Wang, Weile
Saatchi, Sassan
Yu, Yifan
Myneni, Ranga B.
TI Estimation of forest aboveground biomass in California using canopy
height and leaf area index estimated from satellite data
SO REMOTE SENSING OF ENVIRONMENT
LA English
DT Article
DE Aboveground biomass; Leaf area index; Canopy height; Landsat;
Uncertainty assessment
ID SYSTEM DATA RECORD; LAND-COVER; ACCURACY ASSESSMENT; CARBON STOCKS;
LIDAR; SURFACE; EMISSIONS; MODEL; USA; DEFORESTATION
AB Accurate characterization of variability and trends in forest biomass at local to national scales is required for accounting of global carbon sources and sinks and monitoring their dynamics. Here we present a new remote sensing based approach for estimating live forest aboveground biomass (AGB) based on a simple parametric model that combines high-resolution estimates of leaf area index (LAI) from the Landsat Thematic Mapper sensor and canopy maximum height from the Geoscience Laser Altimeter System (GLAS) sensor onboard ICESat, the Ice, Cloud, and land Elevation Satellite. We tested our approach with a preliminary uncertainty assessment over the forested areas of California spanning a broad range of climatic and land-use conditions and find our AGB estimates to be comparable to estimates of AGB from inventory records and other available satellite-estimated AGB maps at aggregated scales. Our study offers a high-resolution approach to map forest aboveground biomass at regional-to-continental scales and assess sources of uncertainties in the estimates. (C) 2014 Elsevier Inc All fights reserved.
C1 [Zhang, Gong; Ganguly, Sangram] NASA, BAERI, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Nemani, Ramakrishna R.] NASA, Adv Supercomp Div, Ames Res Ctr, Moffett Field, CA 94035 USA.
[White, Michael A.] Nat Publishing Grp, San Francisco, CA USA.
[Milesi, Cristina; Hashimoto, Hirofumi; Wang, Weile] Calif State Univ Monterey Bay, NASA, Ames Res Ctr, Dept Sci & Environm Policy, Moffett Field, CA 94035 USA.
[Saatchi, Sassan] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Yu, Yifan] Univ Calif Los Angeles, Dept Atmospher & Ocean Sci, Los Angeles, CA 90095 USA.
[Myneni, Ranga B.] Boston Univ, Dept Earth & Environm, Boston, MA 02215 USA.
RP Zhang, G (reprint author), NASA, BAERI, Ames Res Ctr, Moffett Field, CA 94035 USA.
EM zhanggong07@gmail.com
RI Myneni, Ranga/F-5129-2012;
OI White, Michael/0000-0002-0238-8913
FU Carbon Monitoring System (CMS) program at NASA
FX We acknowledge funding from the Carbon Monitoring System (CMS) program
at NASA. We thank the anonymous reviewers and editors for their
constructive comments and edits to the manuscript. We are particularly
grateful to Dr. Ronald E. McRoberts for all his critical inputs in
improving the manuscript. This research was performed using the NASA
Earth Exchange (NEX) computing facilities.
NR 58
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PU ELSEVIER SCIENCE INC
PI NEW YORK
PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA
SN 0034-4257
EI 1879-0704
J9 REMOTE SENS ENVIRON
JI Remote Sens. Environ.
PD AUG
PY 2014
VL 151
SI SI
BP 44
EP 56
DI 10.1016/j.rse.2014.01.025
PG 13
WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic
Technology
SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science &
Photographic Technology
GA AP7NM
UT WOS:000342264000005
ER
PT J
AU Williams, CA
Collatz, GJ
Masek, J
Huang, CQ
Goward, SN
AF Williams, Christopher A.
Collatz, G. James
Masek, Jeffrey
Huang, Chengquan
Goward, Samuel N.
TI Impacts of disturbance history on forest carbon stocks and fluxes:
Merging satellite disturbance mapping with forest inventory data in a
carbon cycle model framework
SO REMOTE SENSING OF ENVIRONMENT
LA English
DT Article
DE Net ecosystem productivity; Carbon sequestration; Landsat change
detection; Forest inventory and analysis; Conterminous United States
ID COARSE WOODY DEBRIS; WESTERN OREGON; UNITED-STATES; ECOSYSTEM
PRODUCTION; LANDSAT RECORD; BUDGET MODEL; TIME-SERIES; AGE; DYNAMICS;
USA
AB Forest carbon stocks and fluxes are highly dynamic following stand-clearing disturbances from severe fire and harvest and this presents a significant challenge for continental carbon budget assessments. In this work we use forest inventory data to parameterize a carbon cycle model to represent post-disturbance carbon trajectories of carbon pools and fluxes for specific forest types growing in high and low site productivity class settings. We then apply these trajectories to landscapes and regions based on forest age distributions derived from either the FIA data or from Landsat time series stacks (1985-2006) for 54 representative scenes throughout most of the conterminous United States. We estimate the net carbon uptake in forests caused by post-disturbance growth and decomposition ("regrowth sink") for forested regions across the country. At the landscape scale, the prevailing condition of positive net ecosystem productivity (NEP) is in stark contrast to local patches with large sources, particularly in the west where fires and clear cuts create contiguous disturbed patches. At the continental scale, regional differences in disturbance rates reflect management patterns of high disturbance rates in the Southeastern and South Central states, and lower disturbance rates in the Northeast and Northern Lakes States. Despite low contemporary disturbance rates in the Northeast and Northern Lakes States (0.61 and 0.74% y(-1)), the regrowth sink there remains of moderate to large strength (88 and 57 g C m(-2) y(-1)) owing to the continued legacy from historical clearing. Large regrowth sinks are also found in the Southeast, South Central, and Pacific Southwest regions (85, 86, and 95 g C m(2) y(-1)) where disturbance rates also tend to be higher (1.59, 1.38, and 0.93% y(-1)). Overall, the Landsat-derived disturbance rates are elevated relative to FIA-derived rates (1.19 versus 0.93% y(-1)) particularly for western regions. The differences only modestly adjust regional- and continental-scale carbon budgets, reducing NEP from forest regrowth by about 8%. (C) 2013 Elsevier Inc. All rights reserved.
C1 [Williams, Christopher A.] Clark Univ, Grad Sch Geog, Worcester, MA 01610 USA.
[Collatz, G. James; Masek, Jeffrey] NASA, Goddard Space Flight Ctr, Biospher Sci Lab, Greenbelt, MD 20771 USA.
[Huang, Chengquan; Goward, Samuel N.] Univ Maryland, Dept Geog, College Pk, MD 20742 USA.
RP Williams, CA (reprint author), 950 Main St, Worcester, MA 01610 USA.
EM cwilliams@clarku.edu
RI collatz, george/D-5381-2012; Masek, Jeffrey/D-7673-2012;
OI Huang, Chengquan/0000-0003-0055-9798
FU NASA [NNH05ZDA001N]; North American Carbon Program
FX We thank Charles (Chip) Scott and his team at the USFS National
Inventory and Monitoring Applications Center for providing us with FIA
data. We acknowledge the helpful discussions and comments from Warren
Cohen, Richard Houghton, Nancy Thomas, Karen Schleeweis, Robert Kennedy,
Scott Powell, Sean Healey, and Gretchen Moisen, as well as from five
anonymous reviewers. We would also like to thank the organizers of this
Special Issue, including Warren Cohen, Ronald McRoberts, and Dirk
Pflugmacher, for giving us the opportunity to contribute following the
ForestSAT 2012 Conference. This work was funded by NASA NNH05ZDA001N,
North American Carbon Program.
NR 50
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PU ELSEVIER SCIENCE INC
PI NEW YORK
PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA
SN 0034-4257
EI 1879-0704
J9 REMOTE SENS ENVIRON
JI Remote Sens. Environ.
PD AUG
PY 2014
VL 151
SI SI
BP 57
EP 71
DI 10.1016/j.rse.2013.10.034
PG 15
WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic
Technology
SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science &
Photographic Technology
GA AP7NM
UT WOS:000342264000006
ER
PT J
AU Beck, JD
Kinch, M
Sun, XL
AF Beck, Jeffrey D.
Kinch, Mike
Sun, Xiaoli
TI Update on linear mode photon counting with the HgCdTe linear mode
avalanche photodiode
SO OPTICAL ENGINEERING
LA English
DT Article
DE single photon counting; avalanche photodiode; HgCdTe; avalanche
photodiode; mid-wavelength infrared; excess noise factor; photon
detection efficiency; false event rate
ID DIODES
AB The behavior of the gain-voltage characteristic of the mid-wavelength infrared cutoff HgCdTe linear mode avalanche photodiode (e-APD) is discussed both experimentally and theoretically as a function of the width of the multiplication region. Data are shown that demonstrate a strong dependence of the gain at a given bias voltage on the width of the n(-) gain region. Geometrical and fundamental theoretical models are examined to explain this behavior. The geometrical model takes into account the gain-dependent optical fill factor of the cylindrical APD. The theoretical model is based on the ballistic ionization model being developed for the HgCdTe APD. It is concluded that the fundamental theoretical explanation is the dominant effect. A model is developed that combines both the geometrical and fundamental effects. The model also takes into account the effect of the varying multiplication width in the low bias region of the gain-voltage curve. It is concluded that the lower than expected gain seen in the first 2 x 8 HgCdTe linear mode photon counting APD arrays, and higher excess noise factor, was very likely due to the larger than typical multiplication region length in the photon counting APD pixel design. The implications of these effects on device photon counting performance are discussed. (C) 2014 Society of Photo-Optical Instrumentation Engineers (SPIE)
C1 [Beck, Jeffrey D.; Kinch, Mike] DRS Technol Inc, C4ISR Grp, Dallas, TX 75243 USA.
[Sun, Xiaoli] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Beck, JD (reprint author), DRS Technol Inc, C4ISR Grp, 13544 N,Cent Expressway, Dallas, TX 75243 USA.
EM jeff.beck@drs.com
NR 14
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U1 1
U2 11
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 AUG
PY 2014
VL 53
IS 8
AR 081906
DI 10.1117/1.OE.53.8.081906
PG 6
WC Optics
SC Optics
GA AO2YT
UT WOS:000341195300008
ER
PT J
AU Dauler, EA
Grein, ME
Kerman, AJ
Marsili, F
Miki, S
Nam, SW
Shaw, MD
Terai, H
Verma, VB
Yamashita, T
AF Dauler, Eric A.
Grein, Matthew E.
Kerman, Andrew J.
Marsili, Francesco
Miki, Shigehito
Nam, Sae Woo
Shaw, Matthew D.
Terai, Hirotaka
Verma, Varun B.
Yamashita, Taro
TI Review of superconducting nanowire single-photon detector system design
options and demonstrated performance
SO OPTICAL ENGINEERING
LA English
DT Review
DE photodetectors; detector arrays; quantum efficiency; optoelectronic
packaging
ID GIFFORD-MCMAHON CRYOCOOLER; EFFICIENCY; ARRAY
AB We describe a number of methods that have been pursued to develop superconducting nanowire single-photon detectors (SNSPDs) with attractive overall performance, including three systems that operate with >70% system detection efficiency and high maximum counting rates at wavelengths near 1550 nm. The advantages and tradeoffs of various approaches to efficient optical coupling, electrical readout, and SNSPD design are described and contrasted. Optical interfaces to the detectors have been based on fiber coupling, either directly to the detector or through the substrate, using both single-mode and multimode fibers with different approaches to alignment. Recent advances in electrical interfaces have focused on the challenges of scalability and ensuring stable detector operation at high count rates. Prospects for further advances in these and other methods are also described, which may enable larger arrays and higher-performance SNSPD systems in the future. Finally, the use of some of these techniques to develop fully packaged SNSPD systems will be described and the performance available from these recently developed systems will be reviewed. (C) The Authors. Published by SPIE under a Creative Commons Attribution 3.0 Unported License. Distribution or reproduction of this work in whole or in part requires full attribution of the original publication, including its DOI.
C1 [Dauler, Eric A.; Grein, Matthew E.; Kerman, Andrew J.] MIT, Lincoln Lab, Lexington, MA 02420 USA.
[Marsili, Francesco; Shaw, Matthew D.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Miki, Shigehito; Terai, Hirotaka; Yamashita, Taro] Natl Inst Informat & Communicat Technol, Kobe Adv Res Ctr, Nishi Ku, Kobe, Hyogo 6512492, Japan.
[Nam, Sae Woo; Verma, Varun B.] NIST, Boulder, CO 80305 USA.
RP Dauler, EA (reprint author), MIT, Lincoln Lab, 244 Wood St, Lexington, MA 02420 USA.
EM edauler@LL.mit.edu
FU Defense for Research and Engineering under Air Force Contract
[FA8721-05-C-0002]
FX The MIT Lincoln Laboratory portion of this work is sponsored by the
Assistant Secretary of Defense for Research and Engineering under Air
Force Contract FA8721-05-C-0002. Opinions, interpretations, conclusions,
and recommendations are those of the author and are not necessarily
endorsed by the U.S. government. Part of 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 30
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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 AUG
PY 2014
VL 53
IS 8
AR 081907
DI 10.1117/1.OE.53.8.081907
PG 13
WC Optics
SC Optics
GA AO2YT
UT WOS:000341195300009
ER
PT J
AU Cano, Z
Postigo, AD
Pozanenko, A
Butler, N
Thone, CC
Guidorzi, C
Kruhler, T
Gorosabel, J
Jakobsson, P
Leloudas, G
Malesani, D
Hjorth, J
Melandri, A
Mundell, C
Wiersema, K
D'Avanzo, P
Schulze, S
Gomboc, A
Johansson, A
Zheng, W
Kann, DA
Knust, F
Varela, K
Akerlof, CW
Bloom, J
Burkhonov, V
Cooke, E
de Diego, JA
Dhungana, G
Farina, C
Ferrante, FV
Flewelling, HA
Fox, OD
Fynbo, J
Gehrels, N
Georgiev, L
Gonzalez, JJ
Greiner, J
Guver, T
Hatch, N
Jelinek, M
Kehoe, R
Klose, S
Klunko, E
Kopae, D
Kutyrev, A
Krugly, Y
Lee, WH
Levan, A
Linkov, V
Matkin, A
Minikulov, N
Molotov, I
Prochaska, JX
Rieher, MG
Roman-Zuniga, CG
Rumyantsev, V
Sanchez-Ramirez, R
Steele, I
Tanvir, NR
Volnova, A
Watson, AM
Xu, D
Yuan, F
AF Cano, Z.
de Ugarte Postigo, A.
Pozanenko, A.
Butler, N.
Thoene, C. C.
Guidorzi, C.
Kruehler, T.
Gorosabel, J.
Jakobsson, P.
Leloudas, G.
Malesani, D.
Hjorth, J.
Melandri, A.
Mundell, C.
Wiersema, K.
D'Avanzo, P.
Schulze, S.
Gomboc, A.
Johansson, A.
Zheng, W.
Kann, D. A.
Knust, F.
Varela, K.
Akerlof, C. W.
Bloom, J.
Burkhonov, V.
Cooke, E.
de Diego, J. A.
Dhungana, G.
Farina, C.
Ferrante, F. V.
Flewelling, H. A.
Fox, O. D.
Fynbo, J.
Gehrels, N.
Georgiev, L.
Gonzalez, J. J.
Greiner, J.
Guever, T.
Hatch, N.
Jelinek, M.
Kehoe, R.
Klose, S.
Klunko, E.
Kopae, D.
Kutyrev, A.
Krugly, Y.
Lee, W. H.
Levan, A.
Linkov, V.
Matkin, A.
Minikulov, N.
Molotov, I.
Prochaska, J. X.
Rieher, M. G.
Roman-Zuniga, C. G.
Rumyantsev, V.
Sanchez-Ramirez, R.
Steele, I.
Tanvir, N. R.
Volnova, A.
Watson, A. M.
Xu, D.
Yuan, F.
TI A trio of gamma-ray burst supernovae: GRB 120729A, GRB 130215A/SN
2013ez, and GRB 130831A/SN 2013fu
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE gamma-ray burst: general; gamma-ray burst: individual: SN 2013ez;
supernovae: general; supernovae: individual: SN 2013fu
ID DIGITAL SKY SURVEY; CONTINUOUS ENERGY INJECTION; AFTERGLOW LIGHT CURVES;
25 APRIL 1998; HOST GALAXY; MILLISECOND PULSARS; OPTICAL AFTERGLOWS;
IMAGE SUBTRACTION; BRIGHT SUPERNOVA; MAGNETIC-FIELDS
AB We present optical and near-infrared (NIR) photometry for three gamma-ray burst supernovae (GRB-SNe): GRB 120729A, GRB 130215A/SN 2013ez, and GRB 130831A/SN 2013fu. For GRB 130215A/SN 2013ez, we also present optical spectroscopy at t-t(0) = 16.1 d, which covers rest-frame 3000-6250 angstrom. Based on Fell lambda 5169 and Sill lambda 6355, our spectrum indicates an unusually low expansion velocity of similar to 4000-6350 km s(-1), the lowest ever measured for a GRB-SN. Additionally, we determined the brightness and shape of each accompanying SN relative to a template supernova (SN 1998bw), which were used to estimate the amount of nickel produced via nucleosynthesis during each explosion. We find that our derived nickel masses are typical of other GRB-SNe, and greater than those of SNe Ibc that are not associated with GRBs. For GRB 130831A/SN 2013fu, we used our well-sampled R-band light curve (LC) to estimate the amount of ejecta mass and the kinetic energy of the SN, finding that these too are similar to other GRB-SNe. For GRB 130215A, we took advantage of contemporaneous optical/NIR observations to construct an optical/NIR bolometric LC of the afterglow. We fit the bolometric LC with the millisecond magnetar model of Zhang & Meszros (2001, ApJ, 552, L35), which considers dipole radiation as a source of energy injection to the forward shock powering the optical/NIR afterglow. Using this model we derive an initial spin period of P = 12 ms and a magnetic field of B = 1.1 x 10(15) G, which are commensurate with those found for proposed magnetar central engines of other long-duration GRBs.
C1 [Cano, Z.; Jakobsson, P.; Johansson, A.] Univ Iceland, Inst Sci, Ctr Astrophys & Cosmol, IS-107 Reykjavik, Iceland.
[de Ugarte Postigo, A.; Thoene, C. C.; Gorosabel, J.; Jelinek, M.] CSIC, IAA, E-18008 Granada, Spain.
[de Ugarte Postigo, A.; Kruehler, T.; Leloudas, G.; Malesani, D.; Hjorth, J.; Fynbo, J.; Levan, A.; Xu, D.] Niels Bohr Inst, Dark Cosmol Ctr, DK-2100 Copenhagen O, Denmark.
[Pozanenko, A.; Volnova, A.] Space Res Inst, Moscow 117997, Russia.
[Butler, N.] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85287 USA.
[Guidorzi, C.] Univ Ferrara, Dept Phys & Earth Sci, I-44122 Ferrara, Italy.
[Kruehler, T.] European So Observ, Santiago 19, Chile.
[Gorosabel, J.] Univ Pais Vasco UPV EHU, ETS Ingn, Dept Fis Aplicada 1, Unidad Asociada Grp Ciencia Planetarias UPW EHU I, Bilbao 48013, Spain.
[Gorosabel, J.] Basque Fdn Sci, Ikerbasque, Bilbao 48008, Spain.
[Leloudas, G.] Oskar Klein Ctr, S-10691 Stockholm, Sweden.
[Melandri, A.; D'Avanzo, P.] INAF Brera Astron Observ, I-23807 Merate, LC, Italy.
[Mundell, C.; Steele, I.] Liverpool John Moores Univ, Astrophys Res Inst, Liverpool L3 5RF, Merseyside, England.
[Wiersema, K.; Tanvir, N. R.] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England.
[Schulze, S.] Pontificia Univ Catolica Chile, Fac Fis, Inst Astrofis, Macul Santiago 7820436, Chile.
[Schulze, S.] Millennium Ctr Supernova Sci, Santiago, Chile.
[Gomboc, A.; Kopae, D.] Univ Ljubljana, Fac Math & Phys, Ljubljana 1000, Slovenia.
[Zheng, W.; Bloom, J.; Fox, O. D.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA.
[Kann, D. A.; Knust, F.; Varela, K.; Greiner, J.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany.
[Kann, D. A.; Klose, S.] Thuringer Landessternwarte Tautenburg, D-07778 Tautenburg, Germany.
[Akerlof, C. W.] Univ Michigan, Dept Phys, Ann Arbor, MI 48109 USA.
[Burkhonov, V.] Ulugh Beg Astron Inst, Tashkent, Uzbekistan.
[Cooke, E.] Univ Nottingham, Sch Phys & Astron, Nottingham NG7 2RD, England.
[de Diego, J. A.; Georgiev, L.; Gonzalez, J. J.; Lee, W. H.; Roman-Zuniga, C. G.; Watson, A. M.] Univ Nacl Autonoma Mexico, Inst Astron, Mexico City 04510, DF, Mexico.
[Dhungana, G.; Ferrante, F. V.; Kehoe, R.] So Methodist Univ, Dept Phys, Dallas, TX 75275 USA.
[Farina, C.] Isaac Newton Grp Telescopes, Santa Cruz De La Palma 38700, Canary Islands, Spain.
[Flewelling, H. A.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA.
[Gehrels, N.; Kutyrev, A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Guever, T.] Istanbul Univ, Dept Astron & Space Sci, TR-34119 Istanbul, Turkey.
Univ Amsterdam, Astron Inst, NL-1098 XH Amsterdam, Netherlands.
[Hatch, N.] Univ Nottingham, Sch Phys & Astron, Nottingham NG7 2RD, England.
[Klunko, E.] Russian Acad Sci, Inst Solar Terr Phys, Siberian Dept, Irkutsk 664033, Russia.
[Krugly, Y.] Kharkov Natl Univ, Inst Astron, Kharkov, Ukraine.
[Levan, A.] Univ Warwick, Dept Phys, Coventry CV4 7AL, W Midlands, England.
[Linkov, V.] JSC Asron Sci Ctr, Moscow 125362, Russia.
[Matkin, A.] Ussuriysk Astrophys Observ, S Gornotayozhnoe 692533, Russia.
[Minikulov, N.] Acad Sci Tajikistan, Inst Astrophys, Dushanbe 734042, Tajikistan.
[Molotov, I.] Keldysh Inst Appl Math, Moscow, Russia.
[Prochaska, J. X.; Sanchez-Ramirez, R.] Univ Calif Santa Cruz, Dept Astron, Santa Cruz, CA 95064 USA.
[Rieher, M. G.] Univ Nacl Autonoma Mexico, Inst Astron, Ensenada 22800, Baja California, Mexico.
[Rumyantsev, V.] Taras Shevcheriko Natl Univ Kyiv, Crimean Astrophys Observ, Crimea, Ukraine.
[Yuan, F.] Australian Natl Univ, Res Sch Astron & Astrophys, Weston, ACT 2611, Australia.
RP Cano, Z (reprint author), Univ Iceland, Inst Sci, Ctr Astrophys & Cosmol, Dunhagi 5, IS-107 Reykjavik, Iceland.
EM zewcano@gmail.com
RI Jakobsson, Pall/L-9950-2015; Jelinek, Martin/E-5290-2016; Roman-Zuniga,
Carlos/F-6602-2016; Gonzalez, Jose/L-6687-2014;
OI Sanchez-Ramirez, Ruben/0000-0002-7158-5099; Rumyantsev,
Vasilij/0000-0003-1894-7019; Schulze, Steve/0000-0001-6797-1889; Guver,
Tolga/0000-0002-3531-9842; de Ugarte Postigo,
Antonio/0000-0001-7717-5085; Kruehler, Thomas/0000-0002-8682-2384;
Jakobsson, Pall/0000-0002-9404-5650; Jelinek,
Martin/0000-0003-3922-7416; Roman-Zuniga, Carlos/0000-0001-8600-4798;
Gonzalez, Jose/0000-0002-3724-1583; Hatch, Nina/0000-0001-5600-0534;
Thone, Christina/0000-0002-7978-7648
FU Icelandic Research Fund; Danish National Research Foundation; Spanish
research project [AYA2012-39362-C02-02]; European Commission
[FP7-PEOPLE-2012-CIG 322307]; European Commission; ASI [INAF I/004/11/];
RFBR [12-02-01336, 14-02-10015, 13-01-92204]; Max-Planck Institut fur
Extraterrestrische Physik, Garching; Thuringer Landessternwarte
Tautenburg; NASA [NNX13AJ67G, NNX09AH71G, NNX09AT02G, NNX10AI27G,
NNX12AE66G]; ERC-StG [EGGS-278202]; Royal Society; Wolfson Foundation;
Science and Technology Facilities Council; Australian Research Council
Centre of Excellence for All-sky Astrophysics (CAASTRO) [CE110001020];
CONACyT [INFR-2009-01-122785, CB-2008-101958]; UNAM PAPIIT [IN113810];
UC MEXUS-CONACyT [CN 09-283]; CONICYT through FONDECYT [3140534];
Basal-CATA [PFB-06/2007]; Iniciativa Cientifica Milenio [P10-064-F];
Iniciativa Cientifica Milenio del Ministerio de Economa [IC120009];
Fomento y Turismo de Chile; Fondo de Innovacion para la Competitividad,
del Ministerio de Economia, Fomento y Turismo de Chile; DFG [HA
1850/28-1]; [AYA2012-39727-C03-01]
FX I am very grateful to Max de Pasquale for countless discussions
regarding GRB physics, and Antonia Rowlinson for equally stimulating
conversations regarding magnetars. We thank the referee for their
insightful comments on the original manuscript. Z.C. gratefully
acknowledges support by a Project Grant from the Icelandic Research
Fund. The Dark Cosmology Centre is funded by the Danish National
Research Foundation. The research activity of AdUP, CT, RSR, and JGor is
supported by Spanish research project AYA2012-39362-C02-02. J.Gor and
RSR are also supported by project AYA2012-39727-C03-01. AdUP
acknowledges support by the European Commission under the Marie Curie
Career Integration Grant programme (FP7-PEOPLE-2012-CIG 322307). T. K.
acknowledges support by the European Commission under the Marie Curie
Intra-European Fellowship Programme. The research activity of AM and PDA
is supported by ASI grant INAF I/004/11/. A. P, A. V. acknowledge
partial support by RFBR grants 12-02-01336, 14-02-10015, and A. M., I.
M. acknowledge support by RFBR grant 13-01-92204. D. A. K. acknowledges
support by the Max-Planck Institut fur Extraterrestrische Physik,
Garching, and the Thuringer Landessternwarte Tautenburg. J.X.P.
acknowledges support from NASA Swift Grant NNX13AJ67G. J.P.U.F.
acknowledges support from the ERC-StG grant EGGS-278202. Based on
observations made with the Nordic Optical Telescope, operated by the
Nordic Optical Telescope Scientific Association at the Observatorio del
Roque de los Muchachos, La Palma, Spain, of the Instituto de Astrofisica
de Canarias. Based on observations made with the Gran Telescopio
Canarias (GTC), instaled in the Spanish Observatorio del Roque de los
Muchachos of the Instituto de Astrofisica de Canarias, in the island of
La Palma. The Liverpool Telescope is operated by Liverpool John Moores
University at the Observatorio del Roque de los Muchachos of the
Instituto de Astrofisica de Canarias. The Faulkes Telescopes are owned
by Las Cumbres Observatory. C. G. M. acknowledges support from the Royal
Society, the Wolfson Foundation and the Science and Technology
Facilities Council. The ROTSE-IIIb telescope is operated by Southern
Methodist University at McDonald Observatory, Ft. Davis, Texas. Parts of
this research were conducted by the Australian Research Council Centre
of Excellence for All-sky Astrophysics (CAASTRO), through project number
CE110001020. Additionally, we thank the RATIR project team and the staff
of the Observatorio Astronmico Nacional on Sierra San Pedro Martir.
RATIR is a collaboration between the University of California, the
Universidad Nacional Autonoma de Mexico, NASA Goddard Space Flight
Center, and Arizona State University, benefiting from the loan of an
H2RG detector and hardware and software support from Teledyne Scientific
and Imaging. RATIR, the automation of the Harold L. Johnson Telescope of
the Observatorio Astronomico Nacional on Sierra San Pedro Martir, and
the operation of both are funded through NASA grants NNX09AH71G,
NNX09AT02G, NNX10AI27G, and NNX12AE66G, CONACyT grants
INFR-2009-01-122785 and CB-2008-101958, UNAM PAPIIT grant IN113810, and
UC MEXUS-CONACyT grant CN 09-283. S. S.; acknowledges support from
CONICYT through FONDECYT grant 3140534, from Basal-CATA PFB-06/2007,
Iniciativa Cientifica Milenio grant P10-064-F (Millennium Center for
Supernova Science), and by Project IC120009 "Millennium Institute of
Astrophysics (MAS)" of Iniciativa Cientifica Milenio del Ministerio de
Economa, Fomento y Turismo de Chile, with input from "Fondo de
Innovacion para la Competitividad, del Ministerio de Economia, Fomento y
Turismo de Chile". Part of this work is based on observations obtained
at the Gemini Observatory, which is operated by the Association of
Universities for Research in Astronomy, Inc., under a cooperative
agreement with the NSF on behalf of the Gemini partnership: the National
Science Foundation (United States), the National Research Council
(Canada), CONICYT (Chile), the Australian Research Council (Australia),
Ministerio da Ciencia, Tecnologia e Inovacao (Brazil) and Ministerio de
Ciencia, Tecnologia e Innovacion Productiva (Argentina). Part of the
funding for GROND (both hardware as well as personnel) was generously
granted from the Leibniz-Prize to G. Hasinger (DFG grant HA 1850/28-1).
NR 186
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SN 1432-0746
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD AUG
PY 2014
VL 568
AR A19
DI 10.1051/0004-6361/201423920
PG 16
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AO2VZ
UT WOS:000341185900080
ER
PT J
AU Fuente, A
Cernicharo, J
Caselli, P
McCoey, C
Johnstone, D
Fich, M
van Kempen, T
Palau, A
Yildiz, UA
Tercero, B
Lopez, A
AF Fuente, A.
Cernicharo, J.
Caselli, P.
McCoey, C.
Johnstone, D.
Fich, M.
van Kempen, T.
Palau, Aina
Yildiz, U. A.
Tercero, B.
Lopez, A.
TI The hot core towards the intermediate-mass protostar NGC 7129 FIRS 2
Chemical similarities with Orion KL
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE astrochemistry; stars: formation; ISM: individual objects: NGC 7129 FIRS
2
ID LIMITED MILLIMETER SURVEY; GRAIN SURFACE-CHEMISTRY; MOLECULAR LINE
SURVEY; SOLAR-TYPE PROTOSTAR; SUBMILLIMETER ARRAY; TENTATIVE DETECTION;
ROTATIONAL SPECTRUM; ORGANIC-MOLECULES; 1ST DETECTION; SAGITTARIUS B2(N)
AB Context. This paper is dedicated to the study of the chemistry of the intermediate-mass (IM) hot core NGC 7129 FIRS 2, probably the most compact warm core found in the 2-8 M-circle dot stellar mass range.
Aims. Our aim is to determine the chemical composition of the IM hot core NGC 7129 FIRS 2, and to provide new insights on the chemistry of hot cores in a more general context.
Methods. NGC 7129 FIRS 2 (hereafter, FIRS 2) is located at a distance of 1250 pc and high spatial resolution observations are required to resolve the hot core at its center. We present a molecular survey from 218 200 MHz to 221 800 MHz carried out with the IRAM Plateau de Bure Interferometer (PdBI). These observations were complemented with a long integration single-dish spectrum taken with the IRAM 30 m telescope in Pico de Veleta (Spain). We used a local thermodynamic equilibrium (LTE) single temperature code to model the whole dataset.
Results. The interferometric spectrum is crowded with a total of approximate to 300 lines from which a few dozen remain unidentified. The spectrum has been modeled with a total of 20 species and their isomers, isotopologues, and deuterated compounds. Complex molecules like methyl formate (CH3OCHO), ethanol (CH3CH2OH), glycolaldehyde (CH2OHCHO), acetone (CH3COCH3), dimethyl ether (CH3OCH3), ethyl cyanide (CH3CH2CN), and the aGg' conformer of ethylene glycol (aGg'-(CH2OH)(2)) are among the detected species. The detection of vibrationally excited lines of CH3CN, CH3OCHO, CH3OH, OCS, HC3N, and CH3CHO proves the existence of gas and dust at high temperatures. The gas kinetic temperature estimated from the vibrational lines of CH3CN, similar to 405(-67)(+100) K, is similar to that measured in massive hot cores. Our data allow an extensive comparison of the chemistry in FIRS 2 and the Orion hot core.
Conclusions. We find a quite similar chemistry in FIRS 2 and Orion. Most of the studied fractional molecular abundances agree within a factor of 5. Larger differences are only found for the deuterated compounds D2CO and CH2DOH and a few molecules (CH3CH2CN, SO2, HNCO and CH3CHO). Since the physical conditions are similar in both hot cores, only different initial conditions (warmer pre-collapse and collapse phase in the case of Orion) and/or different crossing times of the gas in the hot core can explain this behavior. We discuss these two scenarios.
C1 [Fuente, A.] IGN, Observ Astron Nacl OAN, Alcala De Henares 28803, Spain.
[Cernicharo, J.; Tercero, B.; Lopez, A.] Inst Ciencia Mat Madrid ICMM, Madrid 28049, Spain.
[Caselli, P.] Max Planck Inst Extraterr Phys, D-85741 Garching, Germany.
[McCoey, C.; Fich, M.] Univ Waterloo, Dept Phys & Astron, Waterloo, ON N2L 3G1, Canada.
[Johnstone, D.] Univ Victoria, Dept Phys & Astron, Victoria, BC V8P 1A1, Canada.
[Johnstone, D.] Natl Res Council Canada, Herzberg Inst Astrophys, Victoria, BC V9E 2E7, Canada.
[Johnstone, D.] Joint Astron Ctr, Hilo, HI 96720 USA.
[van Kempen, T.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands.
[Palau, Aina] Univ Nacl Autonoma Mexico, Ctr Radioastron & Astrofis, Morelia 58090, Michoacan, Mexico.
[Yildiz, U. A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Fuente, A (reprint author), IGN, Observ Astron Nacl OAN, Apdo 112, Alcala De Henares 28803, Spain.
EM a.fuente@oan.es
RI Yildiz, Umut/C-5257-2011; Fuente, Asuncion/G-1468-2016
OI Yildiz, Umut/0000-0001-6197-2864; Fuente, Asuncion/0000-0001-6317-6343
FU Spanish MINECO [CSD2009-00038, AYA2009-07304, AYA2012-32032]; National
Research Council of Canada; Natural Sciences and Engineering Research
Council of Canada (NSERC); Spanish MICINN [AYA2011-30228-C03-02]; FEDER
funds; AGAUR (Catalonia) [2009SGR1172]
FX We thank the Spanish MINECO for funding support from grants
CSD2009-00038, AYA2009-07304, and AYA2012-32032. D.J. is supported by
the National Research Council of Canada and by a Natural Sciences and
Engineering Research Council of Canada (NSERC) Discovery Grant. A. P. is
supported by the Spanish MICINN grant AYA2011-30228-C03-02 (co-funded
with FEDER funds), and by the AGAUR grant 2009SGR1172 (Catalonia).
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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
EI 1432-0746
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD AUG
PY 2014
VL 568
AR A65
DI 10.1051/0004-6361/201323074
PG 28
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AO2VZ
UT WOS:000341185900022
ER
PT J
AU Messias, H
Dye, S
Nagar, N
Orellana, G
Bussmann, RS
Calanog, J
Dannerbauer, H
Fu, H
Ibar, E
Inohara, A
Ivison, RJ
Negrello, M
Riechers, DA
Sheen, YK
Aguirre, JE
Amber, S
Birkinshaw, M
Bourne, N
Bradford, CM
Clements, DL
Cooray, A
De Zotti, G
Demarco, R
Dunne, L
Eales, S
Fleuren, S
Kamenetzky, J
Lupu, RE
Maddox, SJ
Marrone, DP
Michalowski, MJ
Murphy, EJ
Nguyen, HT
Omont, A
Rowlands, K
Smith, D
Smith, M
Valiante, E
Vieira, JD
AF Messias, Hugo
Dye, Simon
Nagar, Neil
Orellana, Gustavo
Bussmann, R. Shane
Calanog, Jae
Dannerbauer, Helmut
Fu, Hai
Ibar, Edo
Inohara, Andrew
Ivison, R. J.
Negrello, Mattia
Riechers, Dominik A.
Sheen, Yun-Kyeong
Aguirre, James E.
Amber, Simon
Birkinshaw, Mark
Bourne, Nathan
Bradford, Charles M.
Clements, Dave L.
Cooray, Asantha
De Zotti, Gianfranco
Demarco, Ricardo
Dunne, Loretta
Eales, Stephen
Fleuren, Simone
Kamenetzky, Julia
Lupu, Roxana E.
Maddox, Steve J.
Marrone, Daniel P.
Michalowski, Michal J.
Murphy, Eric J.
Nguyen, Hien T.
Omont, Alain
Rowlands, Kate
Smith, Dan
Smith, Matt
Valiante, Elisabetta
Vieira, Joaquin D.
TI Herschel-ATLAS and ALMA HATLAS J142935.3-002836, a lensed major merger
at redshift 1.027
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE gravitational lensing: strong; galaxies: ISM; galaxies: kinematics and
dynamics
ID STAR-FORMING GALAXIES; SCIENCE DEMONSTRATION PHASE; DEGREE EXTRAGALACTIC
SURVEY; SPITZER-SPACE-TELESCOPE; 1200-MU-M MAMBO SURVEY; DIGITAL SKY
SURVEY; DEEP FIELD-SOUTH; SUBMILLIMETER GALAXIES; MOLECULAR GAS;
INTERSTELLAR-MEDIUM
AB Context. The submillimetre-bright galaxy population is believed to comprise, aside from local galaxies and radio-loud sources, intrinsically active star-forming galaxies, the brightest of which are lensed gravitationally. The latter enable studies at a level of detail beyond what is usually possible by the observation facility.
Aims. This work focuses on one of these lensed systems, HATLAS J142935.3-002836 (H1429-0028), selected in the Herschel-ATLAS field. Gathering a rich, multi-wavelength dataset, we aim to confirm the lensing hypothesis and model the background source's morphology and dynamics, as well as to provide a full physical characterisation.
Methods. Multi-wavelength high-resolution data is utilised to assess the nature of the system. A lensing-analysis algorithm that simultaneously fits different wavebands is adopted to characterise the lens. The background galaxy dynamical information is studied by reconstructing the 3D source plane of the ALMA CO (J: 4 -> 3) transition. Near-IR imaging from HST and Keck-AO allows to constrain rest-frame optical photometry independently for the foreground and background systems. Physical parameters (such as stellar and dust masses) are estimated via modelling of the spectral energy distribution taking source blending, foreground obscuration, and differential magnification into account.
Results. The system comprises a foreground edge-on disk galaxy (at z(sp) = 0.218) with an almost complete Einstein ring around it. The background source (at z(sp) = 1.027) is magnified by a factor of p = 8-10 depending on wavelength. It is comprised of two components and a tens-of-kpc-long tidal tail resembling the Antenna merger. As a whole, the background source is a massive stellar system (1.32(0.41)(+0.63) x 10(11) M.) forming stars at a rate of 394 +/- 90 Mo yr(-1), and it has a significant gas reservoir M-ISM = 4.6 + 1.7 x 10(10) M-circle dot. Its depletion time due to star formation alone is thus expected to be T-sF = M-ISM/SFR = 117 +/- 51 Myr. The dynamical mass of one of the components is estimated to be 5.8 +/- 1.7 x 10(10) M., and, together with the photometric total mass estimate, it implies that H1429-0028 is a major merger system (1: 2.8+ 1).
C1 [Messias, Hugo; Nagar, Neil; Orellana, Gustavo; Sheen, Yun-Kyeong; Demarco, Ricardo] Univ Concepcion, Barrio Univ, Concepcion, Chile.
[Messias, Hugo] Univ Lisbon, Ctr Astron & Astrofis, Observatorio Astron Lisboa, P-1349018 Lisbon, Portugal.
[Dye, Simon; Bourne, Nathan] Univ Nottingham, Sch Phys & Astron, Nottingham NG7 2RD, England.
[Bussmann, R. Shane] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Calanog, Jae; Inohara, Andrew; Cooray, Asantha] Univ Calif Irvine, Dept Phys & Astron, Irvine, CA 92697 USA.
[Dannerbauer, Helmut] Univ Vienna, Inst Astrophys, A-1180 Vienna, Austria.
[Fu, Hai] Univ Iowa, Dept Phys & Astron, Iowa City, IA 52242 USA.
[Ibar, Edo] Univ Valparaiso, Inst Fis & Astron, Valparaiso, Chile.
[Ivison, R. J.; Dunne, Loretta; Maddox, Steve J.; Michalowski, Michal J.] Univ Edinburgh, Inst Astron, Royal Observ, Edinburgh EH9 3HJ, Midlothian, Scotland.
[Ivison, R. J.] European So Observ, Garching, Germany.
[Negrello, Mattia; De Zotti, Gianfranco] Osserv Astron Padova, INAF, I-35122 Padua, Italy.
[Riechers, Dominik A.; Cooray, Asantha] CALTECH, Dept Astron, Pasadena, CA 91125 USA.
[Riechers, Dominik A.] Cornell Univ, Dept Astron, Ithaca, NY 14853 USA.
[Aguirre, James E.; Lupu, Roxana E.] Univ Penn, Dept Phys & Astron, Philadelphia, PA 19104 USA.
[Amber, Simon] Open Univ, Milton Keynes MK7 6BJ, Bucks, England.
[Birkinshaw, Mark] Univ Bristol, HH Wills Phys Lab, Bristol BS8 1TL, Avon, England.
[Birkinshaw, Mark] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Bradford, Charles M.; Nguyen, Hien T.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Clements, Dave L.] Univ London Imperial Coll Sci Technol & Med, Astrophys Grp, Blackett Lab, London SW7 2AZ, England.
[Dunne, Loretta; Maddox, Steve J.] Univ Canterbury, Dept Phys & Astron, Christchurch 8140, New Zealand.
[Eales, Stephen; Smith, Matt; Valiante, Elisabetta] Cardiff Univ, Sch Phys & Astron, Cardiff CF24 3AA, S Glam, Wales.
[Fleuren, Simone] Univ London, Sch Math Sci, London E1 4NS, England.
[Kamenetzky, Julia] Univ Colorado, Ctr Astrophys & Space Astron, Boulder, CO 80309 USA.
[Marrone, Daniel P.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA.
[Murphy, Eric J.] CALTECH, Infrared Proc & Anal Ctr, Pasadena, CA 91125 USA.
[Omont, Alain] Univ Paris 06, Inst Astrophys Paris, UNIR 7095, CNRS, F-75014 Paris, France.
[Rowlands, Kate] Univ St Andrews, SUPA Sch Phys & Astron, St Andrews KY16 9SS, Fife, Scotland.
[Smith, Dan] Univ Hertfordshire, Sci & Technol Res Inst, Ctr Astrophys Res, Hatfield AL10 9AB, Herts, England.
[Vieira, Joaquin D.] Univ Illinois, Dept Astron, Urbana, IL 61801 USA.
[Vieira, Joaquin D.] Univ Illinois, Dept Phys, Urbana, IL 61801 USA.
RP Messias, H (reprint author), Univ Concepcion, Barrio Univ, Concepcion, Chile.
EM hmessias@oal.ul.pt
RI Lupu, Roxana/P-9060-2014; Ivison, R./G-4450-2011;
OI Lupu, Roxana/0000-0003-3444-5908; Ivison, R./0000-0001-5118-1313;
Marrone, Daniel/0000-0002-2367-1080; De Zotti,
Gianfranco/0000-0003-2868-2595; Maddox, Stephen/0000-0001-5549-195X;
Dye, Simon/0000-0002-1318-8343
FU CONYCIT-ALMA [31100008]; FCT [SFRH/BPD/97986/2013,
PTDC/FIS-AST/2194/2012, PEst-OE/FIS/UI2751/2014]; NSF [AST-1313319];
CONICYT/FONDECYT [3130504]; FONDECYT [3130470]; BASAL centre for
Astrophysics and Associated Technologies (CATA) and by FONDECYT
[1130528]
FX H.M. acknowledges the support by CONYCIT-ALMA through a post-doc
scholarship under the project 31100008. HM acknowledges support by FCT
via the post-doctoral fellowship SFRH/BPD/97986/2013 and the programs
PTDC/FIS-AST/2194/2012 and PEst-OE/FIS/UI2751/2014. N.N. and R.D.
acknowledge support from BASAL PFB-06/2007, Fondecyt 1100540 and Anillo
ACT1101. J.A.C. and A. C. acknowledge support from NSF AST-1313319. E.I.
acknowledges funding from CONICYT/FONDECYT postdoctoral project No:
3130504. R.J.I., S.J.M. and L.D. ackowledge support from the European
Research Council in the form of Advanced Investigator grant, COSMICISM.
Y.K.S. acknowledges support by FONDECYT Grant No. 3130470. R.D.
acknowledges the support provided by the BASAL centre for Astrophysics
and Associated Technologies (CATA) and by FONDECYT N. 1130528. K.R.
acknowledges support from the European Research Council Starting Grant
SEDmorph (P.I. Wild). This paper makes use of the following ALMA data:
ADS/JAO. ALMA#2011.0.00476. 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. The National Radio Astronomy Observatory is a
facility of the National Science Foundation operated under cooperative
agreement by Associated Universities, Inc. This publication is based on
data acquired with the Atacama Pathfinder Experiment (APEX). APEX is a
collaboration between the Max-Planck-Institut fur Radioastronomie, the
European Southern Observatory, and the Onsala Space Observatory. We are
grateful to the competent staff at the APEX base-camp in Sequitor, Chile
and the Z-Spec instrument team. Support for CARMA construction was
derived from the Gordon and Betty Moore Foundation, the Kenneth T. and
Eileen L. Norris Foundation, the James S. McDonnell Foundation, the
Associates of the California Institute of Technology, the University of
Chicago, the states of California, Illinois, and Maryland, and the
National Science Foundation. Ongoing CARMA development and operations
are supported by the National Science Foundation under a cooperative
agreement, and by the CARMA partner universities. Based in part on
observations obtained at the Gemini Observatory (include additional
acknowledgement here, see Sect. 1.2), which is operated by the
Association of Universities for Research in Astronomy, Inc., under a
cooperative agreement with the NSF on behalf of the Gemini partnership:
the National Science Foundation (United States), the National Research
Council (Canada), CONICYT (Chile), the Australian Research Council
(Australia), Ministerio da Ciencia, Tecnologia e Inovagao (Brazil) and
Ministerio de Ciencia, Tecnologia e Innovacion Productiva (Argentina).
The Herschel-ATLAS is a project with Herschel, an ESA space observatory
with science instruments provided by European-led Principal Investigator
consortia and with important participation from NASA. The H-ATLAS
website is http://www.h-atlas.org/. Based in part on observations
carried out with the IRAM 30 m Telescope. IRAM is supported by INSU/CNRS
(France), MPG (Germany) and IGN (Spain). Some of the data presented
herein 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 the National Aeronautics and Space
Administration. The Observatory was made possible by the generous
financial support of the W. M. Keck Foundation.; The authors wish to
recognise 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. 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, 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. This work is 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. This publication makes use of data products from the
Wide-field 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. The authors thank the ALMA contact
scientist Adam Leroy for the help throughout scheduling block
preparation and quality assurance, and the help provided by Alexander J.
Conley and Elisabete da Cunha handling, respectively, the MBBEMCEE and
MAGPHYS codes.
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SN 1432-0746
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD AUG
PY 2014
VL 568
AR A92
DI 10.1051/0004-6361/201424410
PG 20
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AO2VZ
UT WOS:000341185900134
ER
PT J
AU Oshagh, M
Santos, NC
Ehrenreich, D
Haghighipour, N
Figueira, P
Santerne, A
Montalto, M
AF Oshagh, M.
Santos, N. C.
Ehrenreich, D.
Haghighipour, N.
Figueira, P.
Santerne, A.
Montalto, M.
TI Impact of occultations of stellar active regions on transmission spectra
Can occultation of a plage mimic the signature of a blue sky?
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE planets and satellites: atmospheres; techniques: photometric; methods:
data analysis; methods: numerical; stars: activity
ID HUBBLE-SPACE-TELESCOPE; EXOPLANET HD 189733B; TIME-SERIES PHOTOMETRY;
SPITZER OBSERVATIONS; EXTRASOLAR PLANET; TRANSITING PLANET; ATMOSPHERIC
HAZE; LIGHT-CURVE; M DWARF; VARIABILITY
AB Transmission spectroscopy during planetary transits, which is based on the measurements of the variations of the planet-to-star radius ratio as a function of wavelength, is a powerful technique to study the atmospheric properties of transiting planets. One of the main limitations of this technique is the effects of stellar activity, which up until now, have been taken into account only by assessing the effect of non-occulted stellar spots on the estimates of the planet-to-star radius ratio. In this paper, we study the impact of the occultation of a stellar spot and plage on the transmission spectra of transiting exoplanets for the first time. We simulated this effect by generating a large number of transit light curves for different transiting planets, stellar spectral types, and different wavelengths. Results of our simulations indicate that the anomalies inside the transit light curve can lead to a significant underestimation or overestimation of the planet-to-star radius ratio as a function of wavelength. At short wavelengths, the effect can reach to a difference of up to 10% in the planet-to-star radius ratio, mimicking the signature of light scattering in the planetary atmosphere. Atmospheric scattering has been proposed to interpret the increasing slopes of transmission spectra toward blue for exoplanets HD 189733b and GJ 3470b. Here, we show that these signatures can be alternatively interpreted by the occultation of stellar plages. Results also suggest that the best strategy to identify and quantify the effects of stellar activities on the transmission spectrum of a planet is to perform several observations during the transit epoch at the same wavelength. This will allow for identifying the possible variations in transit depth as a function of time due to stellar activity variability.
C1 [Oshagh, M.; Santos, N. C.; Figueira, P.; Santerne, A.; Montalto, M.] Univ Porto, Ctr Astrofis, P-4150762 Oporto, Portugal.
[Oshagh, M.; Santos, N. C.] Univ Porto, CAUP, Inst Astrofis & Ciencias Espaco, P-4150762 Oporto, Portugal.
[Oshagh, M.; Santos, N. C.; Figueira, P.; Santerne, A.; Montalto, M.] Univ Porto, Fac Ciencias, Dept Fis & Astron, P-4169007 Oporto, Portugal.
[Ehrenreich, D.] Univ Geneva, Observ Geneve, CH-1290 Sauverny, Switzerland.
[Haghighipour, N.] Univ Hawaii Manoa, Inst Astron, Honolulu, HI 96822 USA.
[Haghighipour, N.] Univ Hawaii Manoa, NASA Astrobiol Inst, Honolulu, HI 96822 USA.
RP Oshagh, M (reprint author), Univ Porto, Ctr Astrofis, Rua Estrelas, P-4150762 Oporto, Portugal.
EM moshagh@astro.up.pt
RI Figueira, Pedro/J-4916-2013; Santos, Nuno/E-9957-2011;
OI Figueira, Pedro/0000-0001-8504-283X; Oshagh,
Mahmoudreza/0000-0002-0715-8789; Santos, Nuno/0000-0003-4422-2919;
Santerne, Alexandre/0000-0002-3586-1316; Ehrenreich,
David/0000-0001-9704-5405
NR 31
TC 18
Z9 18
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
EI 1432-0746
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD AUG
PY 2014
VL 568
AR A99
DI 10.1051/0004-6361/201424059
PG 6
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AO2VZ
UT WOS:000341185900104
ER
PT J
AU Santangelo, G
Nisini, B
Codella, C
Lorenzani, A
Yildiz, UA
Antoniucci, S
Bjerkeli, P
Cabrit, S
Giannini, T
Kristensen, LE
Liseau, R
Mottram, JC
Tafalla, M
van Dishoeck, EF
AF Santangelo, G.
Nisini, B.
Codella, C.
Lorenzani, A.
Yildiz, U. A.
Antoniucci, S.
Bjerkeli, P.
Cabrit, S.
Giannini, T.
Kristensen, L. E.
Liseau, R.
Mottram, J. C.
Tafalla, M.
van Dishoeck, E. F.
TI Water distribution in shocked regions of the NGC 1333-IRAS 4A
protostellar outflow
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE stars: low mass; ISM: jets and outflows; ISM: molecules; ISM: individual
objects: NGC 1333-IRAS 4A; stars: formation
ID STAR-FORMING REGIONS; LOW-MASS PROTOSTARS; YOUNG STELLAR OBJECTS;
HERSCHEL-HIFI; MOLECULAR OUTFLOW; NGC-1333 IRAS-4; KEY PROGRAM; CO
EMISSION; L1157; PACS
AB Context. Water is a key molecule in protostellar environments because its line emission is very sensitive to both the chemistry and the physical conditions of the gas. Observations of H2O line emission from low-mass protostars and their associated outflows performed with HIFI onboard the Herschel Space Observatory have highlighted the complexity of H2O line emission from low-mass protostars and their associated outflows performed with HIFI onboard the Herschel Space Observ line profiles, in which different kinematic components can be distinguished.
Aims. The goal is to study the spatial distribution of H2O line emission from low-mass protostars and their associated outflows performed with HIFI onboard the Herschel Space Observ, in particular of the different kinematic components detected in H2O line emission from low-mass protostars and their associated outflows performed with HIFI onboard the Herschel Space Observ emission, at two bright shocked regions along IRAS 4A, one of the strongest H2O line emission from low-mass protostars and their associated outflows performed with HIFI onboard the Herschel Space Observ emitters among the Class 0 outflows.
Methods. We obtained Herschel-PACS maps of the IRAS 4A outflow and HIFI observations of two shocked positions. The largest HIFI beam of 38'' at 557 GHz was mapped in several key water lines with different upper energy levels, to reveal possible spatial variations of the line profiles. A large velocity gradient (LVG) analysis was performed to determine the excitation conditions of the gas.
Results. We detect four H2O line emission from low-mass protostars and their associated outflows performed with HIFI onboard the Herschel Space Observ lines and CO (16-15) at the two selected shocked positions. In addition, transitions from related outflow and envelope tracers are detected. Different gas components associated with the shock are identified in the H2O emission. In particular, at the head of the red lobe of the outflow, two distinct gas components with different excitation conditions are distinguished in the HIFI emission maps: a compact component, detected in the ground-state water lines, and a more extended one. Assuming that these two components correspond to two different temperature components observed in previous H2O and CO studies, the LVG analysis of the H2O line emission from low-mass protostars and their associated outflows performed with HIFI onboard the Herschel Space Observ emission suggests that the compact (about 32, corresponding to about 700 AU) component is associated with a hot (T similar to 1000 K) gas with densities n(H2) similar to (1-4) x 10(5) cm(-3), whereas the extended (10 ''-17 '', corresponding to 2400-4000 AU) one traces a warm (T similar to 300-500 K) and dense gas (n(H2) similar to (3-5) x 10(7) cm(-3)). Finally, using the CO (16-15) emission observed at R2 and assuming a typical CO/H-2 abundance of 10(-4), we estimate the H2O/H-2 abundance of the warm and hot components to be (7-10) x 10(-7) and (3-7) x 10(-5).
Conclusions. Our data allowed us, for the first time, to resolve spatially the two temperature components previously observed with HIFI and PACS. We propose that the compact hot component may be associated with the jet that impacts the surrounding material, whereas the warm, dense, and extended component originates from the compression of the ambient gas by the propagating flow.
C1 [Santangelo, G.; Codella, C.; Lorenzani, A.] Osserv Astrofis Arcetri, I-50125 Florence, Italy.
[Santangelo, G.; Nisini, B.; Antoniucci, S.; Giannini, T.] Osserv Astron Roma, I-00040 Monte Porzio Catone, Italy.
[Yildiz, U. A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Bjerkeli, P.] Univ Copenhagen, Niels Bohr Inst, DK-2100 Copenhagen O, Denmark.
[Bjerkeli, P.] Univ Copenhagen, Ctr Star & Planet Format, DK-1350 Copenhagen K, Denmark.
[Bjerkeli, P.] Univ Copenhagen, Nat Hist Museum Denmark, DK-1350 Copenhagen K, Denmark.
[Bjerkeli, P.; Liseau, R.] Chalmers, Onsala Space Observ, Dept Earth & Space Sci, S-43992 Onsala, Sweden.
[Cabrit, S.] CNRS, Observ Paris, UMR 8112, LERMA, F-75014 Paris, France.
[Kristensen, L. E.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Mottram, J. C.; van Dishoeck, E. F.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands.
[Tafalla, M.] Observ Astron Nacl IGN, Madrid 28014, Spain.
[van Dishoeck, E. F.] Max Planck Inst Extraterr Phys MPE, D-85748 Garching, Germany.
RP Santangelo, G (reprint author), Osserv Astrofis Arcetri, Largo Enrico Fermi 5, I-50125 Florence, Italy.
EM gina@arcetri.astro.it
RI Yildiz, Umut/C-5257-2011; Kristensen, Lars/F-4774-2011;
OI Giannini, Teresa/0000-0002-0224-096X; , Brunella
Nisini/0000-0002-9190-0113; Yildiz, Umut/0000-0001-6197-2864;
Kristensen, Lars/0000-0003-1159-3721; Lorenzani,
Andrea/0000-0002-4685-3434; Bjerkeli, Per/0000-0002-7993-4118;
Antoniucci, Simone/0000-0002-0666-3847; Codella,
Claudio/0000-0003-1514-3074
FU ASI project [01/005/11/0]
FX Herschel activities at INAF are financially supported by the ASI project
01/005/11/0. HIFI has been designed and built by a consortium of
institutes and university departments from across Europe, Canada and the
United States under the leadership of SRON Netherlands Institute for
Space Research. Groningen, The Netherlands and with major contributions
from Germany, France and the US, Consortium members are Canada: CSA,
U.Waterloo; France; CESR. LAB, LERMA, IRAM: Germany: ROSMA. MPIfR, MPS;
Ireland: NUI Maynooth; Italy: ASI, IFSI-INAF, Osservatorio Astrofisico
di Arcetti- INAF; The Netherlands; SRON, TUD; Poland: CAMK, CHK: Spain:
Observatorio Astronomico Nacional (IGN), Centro de Astrobiologia
(CSIC-INTA): Sweden: Chalmers University of Technology - MC2. RSS &
GARD, Onsala Space Observatory, Swedish National Space Board, Stockholm
University - Stockholm Observatory; Switzerland: ETH Zurich. FHNW: USA;
Caltech, JPL NHSC.
NR 42
TC 8
Z9 8
U1 1
U2 3
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
EI 1432-0746
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD AUG
PY 2014
VL 568
DI 10.1051/0004-6361/201424034
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AO2VZ
UT WOS:000341185900099
ER
PT J
AU Santos-Costa, D
de Pater, I
Sault, RJ
Janssen, MA
Levin, SM
Bolton, SJ
AF Santos-Costa, D.
de Pater, I.
Sault, R. J.
Janssen, M. A.
Levin, S. M.
Bolton, S. J.
TI Multifrequency analysis of the Jovian electron-belt radiation during the
Cassini flyby of Jupiter
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE radiation mechanisms: non-thermal; methods: data analysis
ID SYNCHROTRON-RADIATION; RADIO-EMISSION; 3-DIMENSIONAL RECONSTRUCTION;
RELATIVISTIC ELECTRONS; VLA OBSERVATIONS; SL9 IMPACTS; SOLAR-WIND; GHZ;
CM
AB Aims. We examine Very Large Array (VLA) observations of Jupiter to present evidence of fluctuations in the emission produced by the electron belt in January 2001. Investigating the source of fluctuations will provide new opportunities to discuss the scenarios of temporal changes in Jupiter's synchrotron radiation (i.e., the electron belt) in future data analysis and modeling work.
Methods. To discuss the electron belt dynamics during the Cassini flyby of Jupiter. we compare the radio measurements from 2-3 January 2001 with VLA observations obtained on 20-21 December 1988, when viewing geometry and array configuration are comparable. All data are scaled to a standard Earth-Jupiter distance of 4.04 AU for comparison purposes. Brightness distribution maps with identical spatial resolutions and cartography of the equatorial radiation are constructed and examined at the wavelengths of 21 cm and 90 cm.
Results. Rotation-averaged maps show that the emission from the equatorial zones of maximum intensity is weaker by 5-40%. but the brightness distribution is spatially more extended on 2-3 January 2001. resulting in a total emission at both wavelengths stronger by similar to 35%. Between observation periods, the brightness distributions are observed to evolve differently during the planet rotation. Tomographic reconstructions of the equatorial radiation support our conclusion that the electron belt population was differently distributed around the planet in December 1988 and January 2001.
Conclusions, Our analysis of VLA data sets suggests that the spatial distribution of the electron belt on 2-3 January 2001 is different from that usually observed. Our knowledge of solar activity at the time of the Cassini flyby of Jupiter suggests that the emission from the electron radiation belt was responding to external influences, most likely to solar wind structures rather than to solar radio flux, on a timescale of days to a couple of weeks. Combined results from a multisource data analysis including spacecraft and radio observations are needed to confirm this relationship.
C1 [Santos-Costa, D.; Bolton, S. J.] SW Res Inst, Dept Space Sci, San Antonio, TX 78238 USA.
[de Pater, I.] Univ Calif Berkeley, Berkeley Astron Dept, Berkeley, CA 94720 USA.
[Sault, R. J.] Univ Melbourne, Melbourne, Vic 3010, Australia.
[Janssen, M. A.; Levin, S. M.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
RP Santos-Costa, D (reprint author), SW Res Inst, Dept Space Sci, San Antonio, TX 78238 USA.
EM dsantoscosta@swri.edu; imke@berkeley.edu; rsault@nrao.edu;
michael.janssen@jpl.nasa.gov; steven.m.levin@jpl.nasa.gov;
sbolton@swri.edu
NR 48
TC 3
Z9 3
U1 1
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 1432-0746
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD AUG
PY 2014
VL 568
AR A61
DI 10.1051/0004-6361/201423896
PG 11
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AO2VZ
UT WOS:000341185900077
ER
PT J
AU Sodor, A
Chene, AN
De Cat, P
Bognar, Z
Wright, DJ
Marois, C
Walker, GAH
Matthews, JM
Kallinger, T
Rowe, JF
Kuschnig, R
Guenther, DB
Moffat, AFJ
Rucinski, SM
Sasselov, D
Weiss, WW
AF Sodor, A.
Chene, A. -N.
De Cat, P.
Bognar, Zs.
Wright, D. J.
Marois, C.
Walker, G. A. H.
Matthews, J. M.
Kallinger, T.
Rowe, J. F.
Kuschnig, R.
Guenther, D. B.
Moffat, A. F. J.
Rucinski, S. M.
Sasselov, D.
Weiss, W. W.
TI MOST light-curve analysis of the gamma Doradus pulsator HR 8799, showing
resonances and amplitude variations
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE techniques: photometric; stars: individual: HR 8799; stars: oscillations
ID RR LYRAE STARS; 1ST DETECTION; DEBRIS DISK; VEGA-LIKE; ASTEROSEISMOLOGY;
FREQUENCIES; MODULATION; PHOTOMETRY; MULTISITE; PLANETS
AB Context-The central star of the HR 8799 system is a gamma Dorados-type pulsator. The system harbours four planetary mass companions detected by direct imaging. and is a good solar system analogue. The masses of the companions are not accurately known because the estimation depends greatly on the age of the system, which is also not known with sufficient accuracy. Asteroseisrnic studies of the star might help to better constrain the age of HR 8799. We organized an extensive photometric and multi site spectroscopic observing campaign to study the pulsations of the central star.
Aims. The aim of the present study is to investigate the pulsation properties of HR 8799 in detail via the ultra-precise 47 d nearly continuous photometry obtained with the Microvariability and Oscillations in STars (MOST) space telescope, and to find as many independent pulsation modes as possible, which is the prerequisite for an asteroseismic age determination.
Methods. We carried out Fourier analysis of the wide band photometric time series.
Results. We find that resonance and sudden amplitude changes characterize the pulsation of HR 8799. The dominant frequency is always at f(1) = 1.978 d(-1). Many multiples of one-ninth of the dominant frequency appear in the Fourier spectrum of the MOST data: n/9 f(1). where n =[1, 2, 3, 4. 5, 6,7, 8, 9, 10, 13, 14, 17, 18]. Our analysis also reveals that many of these peaks show strong amplitude decrease and phase variations even on the 47 d time scale. The dependencies between the pulsation frequencies of HR 8799 make the planned subsequent asteroseismic analysis rather difficult We point out some resemblance between the light curve of HR 8799 and the modulated pulsation light curves of Blazhko RR Lyrae stars.
C1 [Sodor, A.; De Cat, P.; Wright, D. J.] Royal Observ Belgium, B-1180 Brussels, Belgium.
[Sodor, A.; Bognar, Zs.] MTA CSFK, Konkoly Observ, H-1121 Budapest, Hungary.
[Chene, A. -N.] Northern Operat Ctr, Gemini Observ, Hilo, HI 96720 USA.
[Wright, D. J.] Univ New S Wales, Sch Phys, Dept Astrophys & Opt, Sydney, NSW 2052, Australia.
[Marois, C.] Natl Res Council Canada, Herzberg Inst Astrophys, Victoria, BC V9E 2E7, Canada.
[Matthews, J. M.] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada.
[Kallinger, T.; Kuschnig, R.; Weiss, W. W.] Univ Vienna, Inst Astron IfA, A-1180 Vienna, Austria.
[Rowe, J. F.] NASA Ames Res Pk, Moffett Field, CA 94035 USA.
[Guenther, D. B.] St Marys Univ, Dept Phys & Astron, Inst Computat Astrophys, Halifax, NS B3H 3C3, Canada.
[Moffat, A. F. J.] Univ Montreal, Dept Phys, Montreal, PQ H3C 3J7, Canada.
[Rucinski, S. M.] Univ Toronto, David Dunlap Observ, Dept Astron & Astrophys, Richmond Hill, ON L4C 4Y6, Canada.
[Sasselov, D.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Sodor, A (reprint author), Royal Observ Belgium, Ringlaan 3, B-1180 Brussels, Belgium.
EM adam.sodor@oma.be
OI Kallinger, Thomas/0000-0003-3627-2561
FU Belgian Federal Science Policy [M0/33/029]; Janos Bolyai Research
Scholarship of the Hungarian Academy of Sciences; Austrian Science Fonds
(EWE) [P22691-N16]
FX A.S. acknowledges support by the Belgian Federal Science Policy (project
M0/33/029, PI: P.D.C.) and by the Janos Bolyai Research Scholarship of
the Hungarian Academy of Sciences. WM. acknowledges support by the
Austrian Science Fonds (EWE) P22691-N16.
NR 26
TC 4
Z9 4
U1 0
U2 0
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
EI 1432-0746
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD AUG
PY 2014
VL 568
AR A106
DI 10.1051/0004-6361/201423976
PG 8
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AO2VZ
UT WOS:000341185900090
ER
PT J
AU Calabrese, E
Hlozek, R
Battaglia, N
Bond, JR
de Bernardis, F
Devlin, MJ
Hajian, A
Henderson, S
Hil, JC
Kosowsky, A
Louis, T
McMahon, J
Moodley, K
Newburgh, L
Niemack, MD
Page, LA
Partridge, B
Sehgal, N
Sievers, JL
Spergel, DN
Staggs, ST
Switzer, ER
Trac, H
Wollack, EJ
AF Calabrese, Erminia
Hlozek, Renee
Battaglia, Nick
Bond, J. Richard
de Bernardis, Francesco
Devlin, Mark J.
Hajian, Amir
Henderson, Shawn
Hil, J. Colin
Kosowsky, Arthur
Louis, Thibaut
McMahon, Jeff
Moodley, Kavilan
Newburgh, Laura
Niemack, Michael D.
Page, Lyman A.
Partridge, Bruce
Sehgal, Neelima
Sievers, Jonathan L.
Spergel, David N.
Staggs, Suzanne T.
Switzer, Eric R.
Trac, Hy
Wollack, Edward J.
TI Precision epoch of reionization studies with next-generation CMB
experiments
SO JOURNAL OF COSMOLOGY AND ASTROPARTICLE PHYSICS
LA English
DT Article
DE CMBR polarisation; CMBR experiments; reionization; Sunyaev-Zeldovich
effect
ID MICROWAVE BACKGROUND POLARIZATION; SELF-REGULATED REIONIZATION;
SOUTH-POLE TELESCOPE; SZ POWER SPECTRUM; SUNYAEV-ZELDOVICH;
INHOMOGENEOUS REIONIZATION; COSMIC REIONIZATION; ANISOTROPIES;
CONSTRAINTS; PROBE
AB Future arcminute resolution polarization data from ground-based Cosmic Microwave Background (CMB) observations can be used to estimate the contribution to the temperature power spectrum from the primary anisotropies and to uncover the signature of reionization near l=1500 in the small angular-scale temperature measurements. Our projections are based on combining expected small-scale E-mode polarization measurements from Advanced ACTPol in the range 300 < l < 3000 with simulated temperature data from the full Planck mission in the low and intermediate l region, 2 < l < 2000 . We show that the six basic cosmological parameters determined from this combination of data will predict the underlying primordial temperature spectrum at high multipoles to better than 1% accuracy. Assuming an efficient cleaning from multi-frequency channels of most foregrounds in the temperature data, we investigate the sensitivity to the only residual secondary component, the kinematic Sunyaev-Zel'dovich (kSZ) term. The CMB polarization is used to break degeneracies between primordial and secondary terms present in temperature and, in effect, to remove from the temperature data all but the residual kSZ term. We estimate a 15 sigma detection of the diffuse homogeneous kSZ signal from expected AdvACT temperature data at l > 1500 , leading to a measurement of the amplitude of matter density fluctuations, sigma(8), at 1% precision. Alternatively, by exploring the reionization signal encoded in the patchy kSZ measurements, we bound the time and duration of the reionization with sigma(z(re)) = 1.1 and sigma(Delta z(re)) = 0.2 . We find that these constraints degrade rapidly with large beam sizes, which highlights the importance of arcminute-scale resolution for future CMB surveys.
C1 [Calabrese, Erminia; Louis, Thibaut] Univ Oxford, Subdept Astrophys, Oxford OX1 3RH, England.
[Hlozek, Renee; Hil, J. Colin; Spergel, David N.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA.
[Battaglia, Nick; Trac, Hy] Carnegie Mellon Univ, Dept Phys, McWilliams Ctr Cosmol, Pittsburgh, PA 15213 USA.
[Bond, J. Richard; Hajian, Amir; Switzer, Eric R.] Univ Toronto, Canadian Inst Theoret Astrophys, Toronto, ON M5S 3H8, Canada.
[de Bernardis, Francesco; Henderson, Shawn; Niemack, Michael D.] Cornell Univ, Dept Phys, Ithaca, NY 14853 USA.
[Devlin, Mark J.] Univ Penn, Dept Phys & Astron, Philadelphia, PA 19104 USA.
[Kosowsky, Arthur] Univ Pittsburgh, Dept Phys & Astron, Pittsburgh, PA 15260 USA.
[McMahon, Jeff] Univ Michigan, Dept Phys, Ann Arbor, MI 48109 USA.
[Moodley, Kavilan] Univ KwaZulu Natal, Sch Math Stat & Comp Sci, Astrophys & Cosmol Res Unit, ZA-4041 Durban, South Africa.
[Newburgh, Laura] Univ Toronto, Dunlap Inst Astron & Astrophys, Toronto, ON M5S 3H4, Canada.
[Page, Lyman A.; Staggs, Suzanne T.] Princeton Univ, Joseph Henry Labs Phys, Princeton, NJ 08544 USA.
[Partridge, Bruce] Haverford Coll, Dept Phys & Astron, Haverford, PA 19041 USA.
[Sehgal, Neelima] SUNY Stony Brook, Dept Phys & Astron, Stony Brook, NY 11794 USA.
[Sievers, Jonathan L.] Univ KwaZulu Natal, Sch Chem & Phys, Astrophys & Cosmol Res Unit, ZA-4041 Durban, South Africa.
[Switzer, Eric R.; Wollack, Edward J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Calabrese, E (reprint author), Univ Oxford, Subdept Astrophys, Keble Rd, Oxford OX1 3RH, England.
EM rminia.calabrese@astro.ox.ac.uk; rhlozek@astro.princeton.edu;
nbattaglia@cmu.edu; bond@cita.utoronto.ca; fd63@cornell.edu;
devlin@dept.physics.upenn.edu; ahajian@cita.utoronto.ca;
swh76@cornell.edu; jhill@iastate.edu; kosowsky@pitt.edu;
thibaut.louis@astro.ox.ac.uk; jeffmcm@umich.edu; moodleyk41@ukzn.ac.za;
newburgh@di.utoronto.ca; niemack@cornell.edu; page@princeton.edu;
bpartrid@haverford.edu; neelima.sehgal@stonybrook.edu;
sieversj@ukzn.ac.za; dns@astro.princeton.edu; staggs@princeton.edu;
eric.r.switzer@nasa.gov; hytrac@cmu.edu; edward.j.wollack@nasa.gov
RI Trac, Hy/N-8838-2014; Wollack, Edward/D-4467-2012;
OI Trac, Hy/0000-0001-6778-3861; Wollack, Edward/0000-0002-7567-4451;
Sievers, Jonathan/0000-0001-6903-5074
FU U.S. National Science Foundation [AST-0408698, AST-0965625]; Princeton
University; University of Pennsylvania; Canada Foundation for Innovation
(CFI); Parque Astronomico Atacama in northern Chile under the auspices
of the Comision Nacional de Investigacion Cientifica y Tecnologica de
Chile (CONICYT); ERC [259505]; NASA ATP [NNX14AB57G]; NSF [AST-
1312991]; [PHY-0855887]; [PHY-1214379]
FX We acknowledge Graeme Addison and Sigurd Naess for useful discussions.
This work was supported by the U.S. National Science Foundation through
awards AST-0408698 and AST-0965625 for the ACT project, as well as
awards PHY-0855887 and PHY-1214379. Funding was also provided by
Princeton University, the University of Pennsylvania, and a Canada
Foundation for Innovation (CFI) award to UBC. ACT operates in the Parque
Astronomico Atacama in northern Chile under the auspices of the Comision
Nacional de Investigacion Cientifica y Tecnologica de Chile (CONICYT).
Funding from ERC grant 259505 supports EC and TL. HT is supported by
grants NASA ATP NNX14AB57G and NSF AST- 1312991. EC thanks Princeton
Astrophysics for hospitality during this work.
NR 63
TC 42
Z9 42
U1 0
U2 3
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 AUG
PY 2014
IS 8
AR 010
DI 10.1088/1475-7516/2014/08/010
PG 21
WC Astronomy & Astrophysics; Physics, Particles & Fields
SC Astronomy & Astrophysics; Physics
GA AP1RM
UT WOS:000341848800010
ER
PT J
AU Raccanelli, A
Bertacca, D
Dore, O
Maartens, R
AF Raccanelli, Alvise
Bertacca, Daniele
Dore, Olivier
Maartens, Roy
TI Large-scale 3D galaxy correlation function and non-Gaussianity
SO JOURNAL OF COSMOLOGY AND ASTROPARTICLE PHYSICS
LA English
DT Article
DE power spectrum; redshift surveys; gravity; cosmological parameters from
LSS
ID PRIMORDIAL NON-GAUSSIANITY; REDSHIFT-SPACE; HALO BIAS; DISTORTIONS
AB We investigate the properties of the 2-point galaxy correlation function at very large scales, including all geometric and local relativistic effects - wide-angle effects, redshift space distortions, Doppler terms and Sachs-Wolfe type terms in the gravitational potentials. The general three-dimensional correlation function has a nonzero dipole and octupole, in addition to the even multipoles of the flat-sky limit. We study how corrections due to primordial non-Gaussianity and General Relativity affect the multipolar expansion, and we show that they are of similar magnitude (when f(NL) is small), so that a relativistic approach is needed. Furthermore, we look at how large-scale corrections depend on the model for the growth rate in the context of modified gravity, and we discuss how a modified growth can affect the non-Gaussian signal in the multipoles.
C1 [Raccanelli, Alvise; Dore, Olivier] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Raccanelli, Alvise; Dore, Olivier] CALTECH, Pasadena, CA 91125 USA.
[Bertacca, Daniele; Maartens, Roy] Univ Western Cape, Dept Phys, ZA-7535 Bellville, South Africa.
[Maartens, Roy] Univ Portsmouth, Inst Cosmol & Gravitat, Portsmouth PO1 3FX, Hants, England.
RP Raccanelli, A (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM alvise@caltech.edu; daniele.bertacca@gmail.com;
Olivier.P.Dore@jpl.nasa.gov; roy.maartens@gmail.com
OI Raccanelli, Alvise/0000-0001-6726-0438; Maartens,
Roy/0000-0001-9050-5894
FU South African Square Kilometre Array Project; South African National
Research Foundation; U.K. Science & Technology Facilities Council
[ST/H002774/1, ST/K0090X/1]
FX We thank Nicola Bartolo, Kazuya Koyama, Marc Manera, Sabino Matarrese,
Will Percival, Ashley Ross, Lado Samushia and Gianmassimo Tasinato for
helpful discussions. Part of 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. The work of DB and RM was supported by the South African
Square Kilometre Array Project and the South African National Research
Foundation. RM was also supported by the U.K. Science & Technology
Facilities Council (grant nos. ST/H002774/1 and ST/K0090X/1).
NR 52
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U1 0
U2 2
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 AUG
PY 2014
IS 8
AR 022
DI 10.1088/1475-7516/2014/08/022
PG 19
WC Astronomy & Astrophysics; Physics, Particles & Fields
SC Astronomy & Astrophysics; Physics
GA AP1RM
UT WOS:000341848800022
ER
PT J
AU Weaver, CP
Mooney, S
Allen, D
Beller-Simms, N
Fish, T
Grambsch, AE
Hohenstein, W
Jacobs, K
Kenney, MA
Lane, MA
Langner, L
Larson, E
McGinnis, DL
Moss, RH
Nichols, LG
Nierenberg, C
Seyller, EA
Stern, PC
Winthrop, R
AF Weaver, C. P.
Mooney, S.
Allen, D.
Beller-Simms, N.
Fish, T.
Grambsch, A. E.
Hohenstein, W.
Jacobs, K.
Kenney, M. A.
Lane, M. A.
Langner, L.
Larson, E.
McGinnis, D. L.
Moss, R. H.
Nichols, L. G.
Nierenberg, C.
Seyller, E. A.
Stern, P. C.
Winthrop, R.
TI From global change science to action with social sciences
SO NATURE CLIMATE CHANGE
LA English
DT Editorial Material
ID CLIMATE ADAPTATION
C1 [Weaver, C. P.; Grambsch, A. E.] US EPA, Washington, DC 20460 USA.
[Mooney, S.] Boise State Univ, Dept Econ, Boise, ID 83725 USA.
[Mooney, S.] Natl Sci Fdn, Expt Program Stimulate Competit Res, Arlington, VA 22230 USA.
[Allen, D.; Seyller, E. A.] US Global Change Res Program, Washington, DC 20006 USA.
[Beller-Simms, N.; Nierenberg, C.] NOAA, Silver Spring, MD 20910 USA.
[Fish, T.] US Dept Interior, Washington, DC 20240 USA.
[Hohenstein, W.] USDA, Washington, DC 20250 USA.
[Jacobs, K.] Univ Arizona, Ctr Climate Adaptat Sci & Solut, Tucson, AZ 85721 USA.
[Jacobs, K.] Univ Arizona, Dept Soil Water & Environm Sci, Tucson, AZ 85721 USA.
[Kenney, M. A.] Univ Maryland, Cooperat Inst Climate & Satellites Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20740 USA.
[Lane, M. A.; Stern, P. C.] CNR, Board Environm Change & Soc, Washington, DC 20001 USA.
[Langner, L.] US Forest Serv, USDA, Washington, DC 20250 USA.
[Larson, E.] NASA, Washington, DC 20546 USA.
[McGinnis, D. L.] Montana State Univ, Billings, MT 59101 USA.
[Moss, R. H.] Pacific NW Natl Lab, Joint Global Change Res Inst, College Pk, MD 20740 USA.
[Moss, R. H.] Univ Maryland, College Pk, MD 20740 USA.
[Nichols, L. G.] Natl Sci Fdn, Div Behav & Cognit Sci, Arlington, VA 22230 USA.
[Winthrop, R.] Bureau Land Management, Washington, DC 20003 USA.
RP Weaver, CP (reprint author), US EPA, 1200 Penn Ave NW, Washington, DC 20460 USA.
EM weaver.chris@epa.gov
RI Weaver, Christopher/G-3714-2010
OI Weaver, Christopher/0000-0003-4016-5451
NR 22
TC 30
Z9 30
U1 1
U2 27
PU NATURE PUBLISHING GROUP
PI LONDON
PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND
SN 1758-678X
EI 1758-6798
J9 NAT CLIM CHANGE
JI Nat. Clim. Chang.
PD AUG
PY 2014
VL 4
IS 8
BP 656
EP 659
PG 4
WC Environmental Sciences; Environmental Studies; Meteorology & Atmospheric
Sciences
SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences
GA AO7YF
UT WOS:000341568200010
ER
PT J
AU Stanford, SA
Gonzalez, AH
Brodwin, M
Gettings, DP
Eisenhardt, PRM
Stern, D
Wylezalek, D
AF Stanford, S. A.
Gonzalez, Anthony H.
Brodwin, Mark
Gettings, Daniel P.
Eisenhardt, Peter R. M.
Stern, Daniel
Wylezalek, Dominika
TI THE MASSIVE AND DISTANT CLUSTERS OF WISE SURVEY. II. INITIAL
SPECTROSCOPIC CONFIRMATION OF z similar to 1 GALAXY CLUSTERS SELECTED
FROM 10,000 deg(2)
SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES
LA English
DT Article
DE galaxies: clusters: individual; galaxies: distances and redshifts;
galaxies: evolution
ID POLE TELESCOPE SURVEY; STELLAR POPULATION SYNTHESIS; DATA RELEASE;
SDSS-III; SPITZER; IRAC; EVOLUTION; DISCOVERY; UNIVERSE; SAMPLE
AB We present optical and infrared imaging and optical spectroscopy of galaxy clusters which were identified as part of an all-sky search for high-redshift galaxy clusters, the Massive and Distant Clusters of WISE Survey (MaDCoWS). The initial phase of MaDCoWS combined infrared data from the all-sky data release of the Wide-field Infrared Survey Explorer (WISE) with optical data from the Sloan Digital Sky Survey to select probable z similar to 1 clusters of galaxies over an area of 10,000 deg(2). Our spectroscopy confirms 19 new clusters at 0.7 < z < 1.3, half of which are at z > 1, demonstrating the viability of using WISE to identify high-redshift galaxy clusters. The next phase of MaDCoWS will use the greater depth of the AllWISE data release to identify even higher redshift cluster candidates.
C1 [Stanford, S. A.] Univ Calif Davis, Dept Phys, Davis, CA 95616 USA.
[Stanford, S. A.] Lawrence Livermore Natl Lab, Inst Geophys & Planetary Phys, Livermore, CA 94550 USA.
[Gonzalez, Anthony H.; Gettings, Daniel P.] Univ Florida, Dept Astron, Bryant Space Ctr 211, Gainesville, FL 32611 USA.
[Brodwin, Mark] Univ Missouri, Dept Phys & Astron, Kansas City, MO 64110 USA.
[Eisenhardt, Peter R. M.; Stern, Daniel] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Wylezalek, Dominika] European So Observ, D-85748 Garching, Germany.
RP Stanford, SA (reprint author), Univ Calif Davis, Dept Phys, One Shields Ave, Davis, CA 95616 USA.
FU Alfred P. Sloan Foundation; National Science Foundation; U.S. Department
of Energy Office of Science; NASA Astrophysics Data Analysis Program
(ADAP) [NNX12AE15G]; W.M. Keck Foundation
FX This publication makes use of data products from the Wide-field 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 (NASA). Funding for SDSS-III has been provided by the
Alfred P. Sloan Foundation, the Participating Institutions, the National
Science Foundation, and the U.S. 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, a list of which can be found at
https://www.sdss3.org/collaboration/institutions.php. We acknowledge
using EzGal, available at www.baryons.org/ezgal/index.php, to calculate
the colors displayed in the color-magnitude diagrams. S.A.S, M.B.,
D.P.G., and A.H.G. acknowledge support for this research from the NASA
Astrophysics Data Analysis Program (ADAP) through grant NNX12AE15G. Some
of the data presented herein 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 the National
Aeronautics and Space Administration. The Observatory was made possible
by the generous financial support of the W.M. Keck Foundation. A.H.G and
D.P.G. were Visiting Astronomers at Gemini Observatory, National Optical
Astronomy Observatory, which is operated by the Association of
Universities for Research in Astronomy (AURA) under cooperative
agreement with the National Science Foundation. This work is 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. Based on observations made with
the Gran Telescopio Canarias (GTC), installed in the Spanish
Observatorio del Roque de los Muchachos of the Instituto de Astrofsica
de Canarias, on the island of La Palma. We thank the anonymous referee
for comments which improved the final manuscript.
NR 35
TC 12
Z9 12
U1 0
U2 1
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0067-0049
EI 1538-4365
J9 ASTROPHYS J SUPPL S
JI Astrophys. J. Suppl. Ser.
PD AUG
PY 2014
VL 213
IS 2
AR 25
DI 10.1088/0067-0049/213/2/25
PG 14
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AP0TM
UT WOS:000341777400007
ER
PT J
AU Vrsnak, B
Temmer, M
Zic, T
Taktakishvili, A
Dumbovic, M
Mostl, C
Veronig, AM
Mays, ML
Odstrcil, D
AF Vrsnak, B.
Temmer, M.
Zic, T.
Taktakishvili, A.
Dumbovic, M.
Moestl, C.
Veronig, A. M.
Mays, M. L.
Odstrcil, D.
TI HELIOSPHERIC PROPAGATION OF CORONAL MASS EJECTIONS: COMPARISON OF
NUMERICAL WSA-ENLIL plus CONE MODEL AND ANALYTICAL DRAG-BASED MODEL
SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES
LA English
DT Article
DE magnetohydrodynamics (MHD); methods: analytical; methods: numerical;
methods: statistical; solar-terrestrial relations; solar wind; Sun:
coronal mass ejections (CMEs)
ID AERODYNAMIC DRAG; SOLAR-WIND; ARRIVAL TIMES; CURRENT SHEET; 1 AU; EARTH;
DYNAMICS; KINEMATICS; PLASMA; CMES
AB Real-time forecasting of the arrival of coronal mass ejections (CMEs) at Earth, based on remote solar observations, is one of the central issues of space-weather research. In this paper, we compare arrival-time predictions calculated applying the numerical "WSA-ENLIL+Cone model" and the analytical "drag-based model" (DBM). Both models use coronagraphic observations of CMEs as input data, thus providing an early space-weather forecast two to four days before the arrival of the disturbance at the Earth, depending on the CME speed. It is shown that both methods give very similar results if the drag parameter Gamma = 0.1 is used in DBM in combination with a background solar-wind speed of w = 400 km s(-1). For this combination, the mean value of the difference between arrival times calculated by ENLIL and DBM is (Delta) over bar = 0.09 +/- 9.0 hr with an average of the absolute-value differences of vertical bar Delta vertical bar = 7.1 hr. Comparing the observed arrivals (O) with the calculated ones (C) for ENLIL gives O - C = -0.3 +/- 16.9 hr and, analogously, O - C = +1.1 +/- 19.1 hr for DBM. Applying Gamma = 0.2 with w = 450 km s(-1) in DBM, one finds O - C = - 1.7 +/- 18.3 hr, with an average of the absolute-value differences of 14.8 hr, which is similar to that for ENLIL, 14.1 hr. Finally, we demonstrate that the prediction accuracy significantly degrades with increasing solar activity.
C1 [Vrsnak, B.; Zic, T.; Dumbovic, M.] Univ Zagreb, Fac Geodesy, Hvar Observ, HR-10000 Zagreb, Croatia.
[Temmer, M.; Moestl, C.; Veronig, A. M.] Graz Univ, Inst Phys, Kanzelhohe Observ IGAM, A-8010 Graz, Austria.
[Taktakishvili, A.; Mays, M. L.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Taktakishvili, A.; Mays, M. L.] Catholic Univ Amer, Washington, DC 20064 USA.
[Moestl, C.] Austrian Acad Sci, Space Res Inst, A-8042 Graz, Austria.
[Odstrcil, D.] George Mason Univ, Fairfax, VA 22030 USA.
RP Vrsnak, B (reprint author), Univ Zagreb, Fac Geodesy, Hvar Observ, Kacceva 26, HR-10000 Zagreb, Croatia.
EM bvrsnak@geof.hr; manuela.temmer@uni-graz.at; tzic@geof.hr;
aleksandre.taktakishvili-1@nasa.gov; mdumbovic@geof.hr;
christian.moestl@uni-graz.at; astrid.veronig@uni-graz.at;
m.leila.mays@nasa.gov; dusan.odstrcil@nasa.gov
RI Veronig, Astrid/B-8422-2009;
OI Zic, Tomislav/0000-0001-6372-8013; Temmer, Manuela/0000-0003-4867-7558;
Moestl, Christian/0000-0001-6868-4152
FU European Commission's Seventh Framework Programme (FP7) [263252,
284461]; Austrian Science Fund (FWF) [V195-N16, P26174-N27]; Shota
Rustaveli Foundation, Georgian National Science Foundation
[DI/14/6-310/12]; Marie Curie International Outgoing Fellowship within
the 7th European Community Framework Programme
FX The research leading to these results has received funding from the
European Commission's Seventh Framework Programme (FP7/2007-2013) under
the grant agreement No. 263252 (COMESEP; www.comesep.eu) and No. 284461
(eHEROES; http://soteria-space.eu/eheroes/html/). M.T., A.V., and C.M.
thank the Austrian Science Fund (FWF): V195-N16 and P26174-N27. A.T.
greatly acknowledges Shota Rustaveli Foundation, Georgian National
Science Foundation grant DI/14/6-310/12. This research was supported by
a Marie Curie International Outgoing Fellowship within the 7th European
Community Framework Programme.
NR 39
TC 15
Z9 15
U1 2
U2 8
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0067-0049
EI 1538-4365
J9 ASTROPHYS J SUPPL S
JI Astrophys. J. Suppl. Ser.
PD AUG
PY 2014
VL 213
IS 2
AR 21
DI 10.1088/0067-0049/213/2/21
PG 9
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AP0TM
UT WOS:000341777400003
ER
PT J
AU McClelland, M
Campbell, M
Estlin, T
AF McClelland, Mark
Campbell, Mark
Estlin, Tara
TI Qualitative Relational Mapping for Mobile Robots with Minimal Sensing
SO JOURNAL OF AEROSPACE INFORMATION SYSTEMS
LA English
DT Article
ID SIMULTANEOUS LOCALIZATION; NAVIGATION; SLAM; INFORMATION; MAP;
CONSISTENCY; ORIENTATION; SPACE
AB This paper presents a novel method for autonomous robotic navigation and mapping of large-scale spaces with minimal sensing. The proposed algorithm constructs a graph-based map that encodes the relative location of landmarks in the environment. Uncertainty in these locations is captured by imposing qualitative constraints on the relationships between landmarks observed by the robot. These relationships are represented in terms of the relative geometrical layout of landmark triplets. A novel measurement method based on camera imagery is presented that extends previous work from the field of qualitative spatial reasoning. Measurements are fused into the map using a deterministic approach based on iterative graph updates. The generation of these maps does not depend on estimates of robot egomotion, and it is consequently suitable for high-slip environments. Algorithm performance is evaluated using MonteCarlo simulations, and results are presented for an experiment using data gathered in the Jet Propulsion Laboratory, California Institute of Technology MarsYard.
C1 [McClelland, Mark] Cornell Univ, Dept Mech & Aerosp Engn, Ithaca, NY 14853 USA.
[Campbell, Mark] Cornell Univ, Sibley Sch Mech & Aerosp Engn, Dept Mech & Aerosp Engn, Ithaca, NY 14853 USA.
[Estlin, Tara] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP McClelland, M (reprint author), Cornell Univ, Dept Mech & Aerosp Engn, Ithaca, NY 14853 USA.
EM mjm496@cornell.edu; mc288@cornell.edu; Tara.Estlin@jpl.nasa.gov
RI Campbell, Mark/F-8312-2013
OI Campbell, Mark/0000-0003-0775-4297
FU NASA Graduate Student Research Program; Cornell University; Jet
Propulsion Laboratory, California Institute of Technology
FX The research presented in this paper has been supported by a fellowship
from the NASA Graduate Student Research Program. This work was performed
by Cornell University and by the Jet Propulsion Laboratory, California
Institute of Technology, under contract with NASA.
NR 25
TC 1
Z9 1
U1 0
U2 2
PU AMER INST AERONAUTICS ASTRONAUTICS
PI RESTON
PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA
SN 1940-3151
EI 2327-3097
J9 J AEROSP INFORM SYST
JI J. Aerosp. Inf. Syst.
PD AUG
PY 2014
VL 11
IS 8
BP 497
EP 511
DI 10.2514/1.I010155
PG 15
WC Engineering, Aerospace
SC Engineering
GA AP0YI
UT WOS:000341792200002
ER
PT J
AU Pugh-Thomas, D
AF Pugh-Thomas, Devin
TI Spectroscopic properties and Judd-Ofelt analysis of BaY2F8:Sm3+
SO JOURNAL OF THE OPTICAL SOCIETY OF AMERICA B-OPTICAL PHYSICS
LA English
DT Article
ID RARE-EARTH IONS; SPECTRAL PROPERTIES; OPTICAL-ABSORPTION;
SINGLE-CRYSTALS; LBTAF GLASSES; LASER; SM3+; PHOTOLUMINESCENCE;
INTENSITIES; CONVERSION
AB Optical spectroscopy and Judd-Ofelt analysis were performed on a BaY2F8:Sm3+ crystal and used to guide the potential application of BaY2F8:Sm3+ as a laser material. Crystals were characterized by polarized absorption spectroscopy, fluorescence emission, and fluorescence lifetime measurements. The H-6(9/2) and H-6(7/2) manifolds are of most interest for visible lasers. This investigation seeks to capture the behavior of the samarium ion in a barium-yttrium-fluoride host from the UV-vis into the near-infrared wavelength regions. (C) 2014 Optical Society of America
C1 NASA, Langley Res Ctr, Hampton, VA 23681 USA.
RP Pugh-Thomas, D (reprint author), NASA, Langley Res Ctr, Hampton, VA 23681 USA.
EM devin.pugh-thomas@nasa.gov
FU NASA Internal Research and Development Fund
FX Appreciation is extended to Drs. Brian M. Walsh and Archie L. Holmes for
helpful discussions. Appreciation is extended to Dr. Arlete Cassanho of
A.C. Materials for information on crystal growth. This investigation was
supported by the NASA Internal Research and Development Fund.
NR 31
TC 1
Z9 1
U1 3
U2 9
PU OPTICAL SOC AMER
PI WASHINGTON
PA 2010 MASSACHUSETTS AVE NW, WASHINGTON, DC 20036 USA
SN 0740-3224
EI 1520-8540
J9 J OPT SOC AM B
JI J. Opt. Soc. Am. B-Opt. Phys.
PD AUG
PY 2014
VL 31
IS 8
BP 1777
EP 1785
DI 10.1364/JOSAB.31.001777
PG 9
WC Optics
SC Optics
GA AO8FU
UT WOS:000341589700005
ER
PT J
AU Ting, WJ
Chang, CH
Chen, SE
Chen, HC
Shy, JT
Drouin, BJ
Daly, AM
AF Ting, Wei-Jo
Chang, Chun-Hung
Chen, Shih-En
Chen, Hsuan-Chen
Shy, Jow-Tsong
Drouin, Brian J.
Daly, Adam M.
TI Precision frequency measurement of N2O transitions near 4.5 mu m and
above 150 mu m
SO JOURNAL OF THE OPTICAL SOCIETY OF AMERICA B-OPTICAL PHYSICS
LA English
DT Article
ID QUANTUM-CASCADE-LASER; NITROUS-OXIDE; ABSORPTION SPECTROSCOPY;
ROTATIONAL TRANSITIONS; DIRECT LINK; COMB; MICROWAVE; SPECTRUM;
SUBMILLIMETER; SPECTROMETER
AB Frequency measurements are given for the 10(0)0 <-- 00(0)0 band of N2O near 4.5 mu m and for pure rotational transitions beyond 151.5 mu m. The infrared measurements utilize a periodically poled lithium niobate (PPLN) based difference frequency generation (DFG) source locked to the saturated absorption center of an N2O absorption line. The DFG frequency is calibrated by an optical frequency comb and an iodine hyperfine transition. We report 44 transitions ranging from J = 1 - 100 for both the P and R branches and the accuracy is better than 10 kHz for most transitions. In addition, 175 pure rotational transitions have been measured including 33 measurements with sub-Doppler precision (<= 3 kHz), and 142 Doppler limited measurements. These are combined with other precision rotational and vibrational measurements to provide improved quantum mechanical parameters, as well as frequency calibration tables for the N2O bands near 4.5 mu m. (C) 2014 Optical Society of America
C1 [Ting, Wei-Jo; Chang, Chun-Hung; Chen, Shih-En; Shy, Jow-Tsong] Natl Tsing Hua Univ, Dept Phys, Hsinchu 30013, Taiwan.
[Chen, Hsuan-Chen; Shy, Jow-Tsong] Natl Tsing Hua Univ, Inst Photon Technol, Hsinchu 30013, Taiwan.
[Shy, Jow-Tsong] Natl Tsing Hua Univ, Frontier Res Ctr Fundamental & Appl Sci Matters, Hsinchu 30013, Taiwan.
[Drouin, Brian J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Shy, JT (reprint author), Natl Tsing Hua Univ, Dept Phys, Hsinchu 30013, Taiwan.
EM shy@phys.nthu.edu.tw
FU National Science Council; Ministry of Education of Taiwan; National
Aeronautics and Space Administration
FX The research at NTHU is supported by the National Science Council and
the Ministry of Education of Taiwan. Portions of this research were
carried out at the Jet Propulsion Laboratory, California Institute of
Technology, under contract with the National Aeronautics and Space
Administration.
NR 51
TC 2
Z9 2
U1 5
U2 18
PU OPTICAL SOC AMER
PI WASHINGTON
PA 2010 MASSACHUSETTS AVE NW, WASHINGTON, DC 20036 USA
SN 0740-3224
EI 1520-8540
J9 J OPT SOC AM B
JI J. Opt. Soc. Am. B-Opt. Phys.
PD AUG
PY 2014
VL 31
IS 8
BP 1954
EP 1963
DI 10.1364/JOSAB.31.001954
PG 10
WC Optics
SC Optics
GA AO8FU
UT WOS:000341589700030
ER
PT J
AU Moore, AD
Downs, ME
Lee, SMC
Feiveson, AH
Knudsen, P
Ploutz-Snyder, L
AF Moore, Alan D., Jr.
Downs, Meghan E.
Lee, Stuart M. C.
Feiveson, Alan H.
Knudsen, Poul
Ploutz-Snyder, Lori
TI Peak exercise oxygen uptake during and following long-duration
spaceflight
SO JOURNAL OF APPLIED PHYSIOLOGY
LA English
DT Article
DE aerobic capacity; weightlessness; International Space Station
ID MANNED SKYLAB MISSION; MIDDLE-AGED MEN; RED-BLOOD-CELL; BED-REST;
CARDIOVASCULAR-RESPONSES; CARDIAC ATROPHY; SPACE-FLIGHT; ORTHOSTATIC
INTOLERANCE; MAXIMAL EXERCISE; EXPERIMENT M-171
AB This investigation was designed to measure aerobic capacity ((V) over dot O-2peak) during and after long-duration International Space Station (ISS) missions. Astronauts (9 males, 5 females: 49 +/- 5 yr, 77.2 +/- 15.1 kg, 40.6 +/- 6.4 ml.kg(-1).min (-1) [mean +/- SD]) performed peak cycle tests similar to 90 days before flight, 15 days after launch, every similar to 30 days in-flight, and on recovery days 1 (R + 1), R + 10, and R + 30. Expired metabolic gas fractions, ventilation, and heart rate (HR) were measured. Data were analyzed using mixed-model linear regression. The main findings of this study were that (V) over dot O-2peak decreased early in-flight (similar to 17%) then gradually increased during flight but never returned to preflight levels. (V) over dot O-2peak was lower on R + 1 and R + 10 than preflight but recovered by R + 30. Peak HR was not different from preflight at any time during or following flight. A sustained decrease in (V) over dot O-2peak during and/or early postflight was not a universal finding in this study, since seven astronauts were able to attain their preflight (V) over dot O-2peak levels either at some time during flight or on R + 1. Four of these astronauts performed in-flight exercise at higher intensities compared with those who experienced a decline in (V) over dot O-2peak , and three had low aerobic capacities before flight. These data indicate that, while (V) over dot O-2peak may be difficult to maintain during long-duration ISS missions, aerobic deconditioning is not an inevitable consequence of long-duration spaceflight.
C1 [Moore, Alan D., Jr.; Lee, Stuart M. C.] Technol & Engn Grp, Houston, TX USA.
[Downs, Meghan E.] Univ Houston, Houston, TX USA.
[Feiveson, Alan H.] NASA, Johnson Space Ctr, Houston, TX USA.
[Knudsen, Poul] Danish Aerosp Co, Odense, Denmark.
[Ploutz-Snyder, Lori] Univ Space Res Assoc, Houston, TX USA.
RP Downs, ME (reprint author), Mail Code SK,1290 Hercules Ave, Houston, TX 77058 USA.
EM meghan.e.everett@nasa.gov
FU NASA Human Research Program
FX This research was supported by the NASA Human Research Program.
NR 48
TC 16
Z9 17
U1 1
U2 14
PU AMER PHYSIOLOGICAL SOC
PI BETHESDA
PA 9650 ROCKVILLE PIKE, BETHESDA, MD 20814 USA
SN 8750-7587
EI 1522-1601
J9 J APPL PHYSIOL
JI J. Appl. Physiol.
PD AUG 1
PY 2014
VL 117
IS 3
BP 231
EP 238
DI 10.1152/japplphysiol.01251.2013
PG 8
WC Physiology; Sport Sciences
SC Physiology; Sport Sciences
GA AO4LK
UT WOS:000341309400005
PM 24970852
ER
PT J
AU Rauscher, BJ
Boehm, N
Cagiano, S
Delo, GS
Foltz, R
Greenhouse, MA
Hickey, M
Hill, RJ
Kan, E
Lindler, D
Mott, DB
Waczynski, A
Wen, YT
AF Rauscher, Bernard J.
Boehm, Nicholas
Cagiano, Steve
Delo, Gregory S.
Foltz, Roger
Greenhouse, Matthew A.
Hickey, Michael
Hill, Robert J.
Kan, Emily
Lindler, Don
Mott, D. Brent
Waczynski, Augustyn
Wen, Yiting
TI New and Better Detectors for the JWST Near-Infrared Spectrograph
SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF THE PACIFIC
LA English
DT Article
ID WEBB-SPACE-TELESCOPE
AB ESA and NASA recently selected two 5 mu m cutoff Teledyne H2RG sensor chip assemblies (S CA) for flight on the James Webb Space Telescope (JWST) Near Infrared Spectrograph (NIRSpec). These HgCdTe SCAs incorporate Teledyne's "improved barrier layer" design that eliminates the degradation that affected earlier JWST H2RGs. The better indium barrier, together with other design changes that Teledyne phased in from other programs over the years, has improved the performance and reliability of JWST's SCAs. In this article, we describe the measured performance characteristics that most directly affect scientific observations including read noise, total noise, dark current, quantum efficiency (QE), and image persistence. As part of measuring QE, we inferred the quantum yield over the full NIRSpec pass band of lambda = 0.6-5 mu m and found that it exceeds unity for photon energies E-gamma > (2.65 +/- .2)E-g, where E-g is the HgCdTe bandgap energy. This corresponds to lambda less than or similar to 2 mu m for NIRSpec's 5 mu m cutoff HgCdTe.
C1 [Rauscher, Bernard J.; Cagiano, Steve; Foltz, Roger; Greenhouse, Matthew A.; Hickey, Michael; Kan, Emily; Mott, D. Brent; Waczynski, Augustyn; Wen, Yiting] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Boehm, Nicholas; Delo, Gregory S.] Global Sci & Technol Inc GST, Greenbelt, MD 20770 USA.
[Hill, Robert J.] Conceptual Analyt LLC, Glenn Dale, MD USA.
[Lindler, Don] Sigma Space Corp, Lanham, MD 20706 USA.
RP Rauscher, BJ (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
EM Bernard.J.Rauscher@nasa.gov
FU NASA
FX This work was supported by NASA as part of the James Webb Space
Telescope Project. We are very grateful to John Auyeung, who manages
JWST work at Teledyne, and to Eric Piquette, our HgCdTe lead at
Teledyne. Both did a fantastic job making the new detectors possible! We
also wish to thank Drs. Mike Regan and Peter McCullough of the Space
Telescope Science Institute (STScI), both of whom read the manuscript
and provided valuable feedback.
NR 22
TC 10
Z9 10
U1 2
U2 7
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-6280
EI 1538-3873
J9 PUBL ASTRON SOC PAC
JI Publ. Astron. Soc. Pac.
PD AUG
PY 2014
VL 126
IS 942
BP 739
EP 749
PG 11
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AO3KH
UT WOS:000341227600002
ER
PT J
AU Pinzon, JE
Tucker, CJ
AF Pinzon, Jorge E.
Tucker, Compton J.
TI A Non-Stationary 1981-2012 AVHRR NDVI3g Time Series
SO REMOTE SENSING
LA English
DT Article
DE Advanced Very High Resolution Radiometer (AVHRR); Normalized Difference
Vegetation Index (NDVI); Bayesian analysis; uncertainty; bias; climate
variability; non-stationary
ID HIGH-RESOLUTION RADIOMETER; NEAR-INFRARED CHANNELS; LAND DATA SET;
SATELLITE DATA; INTERSATELLITE CALIBRATION; MONITORING VEGETATION;
TROPOSPHERIC AEROSOL; ARCTIC TUNDRA; GLOBAL DATA; DATA RECORD
AB The NDVI3g time series is an improved 8-km normalized difference vegetation index (NDVI) data set produced from Advanced Very High Resolution Radiometer (AVHRR) instruments that extends from 1981 to the present. The AVHRR instruments have flown or are flying on fourteen polar-orbiting meteorological satellites operated by the National Oceanic and Atmospheric Administration (NOAA) and are currently flying on two European Organization for the Exploitation of Meteorological Satellites (EUMETSAT) polar-orbiting meteorological satellites, MetOp-A and MetOp-B. This long AVHRR record is comprised of data from two different sensors: the AVHRR/2 instrument that spans July 1981 to November 2000 and the AVHRR/3 instrument that continues these measurements from November 2000 to the present. The main difficulty in processing AVHRR NDVI data is to properly deal with limitations of the AVHRR instruments. Complicating among-instrument AVHRR inter-calibration of channels one and two is the dual gain introduced in late 2000 on the AVHRR/3 instruments for both these channels. We have processed NDVI data derived from the Sea-Viewing Wide Field-of-view Sensor (SeaWiFS) from 1997 to 2010 to overcome among-instrument AVHRR calibration difficulties. We use Bayesian methods with high quality well-calibrated SeaWiFS NDVI data for deriving AVHRR NDVI calibration parameters. Evaluation of the uncertainties of our resulting NDVI values gives an error of +/- 0.005 NDVI units for our 1981 to present data set that is independent of time within our AVHRR NDVI continuum and has resulted in a non-stationary climate data set.
C1 [Pinzon, Jorge E.] NASA, Goddard Space Flight Ctr, Sci Syst & Applicat Inc, Biospher Sci Lab, Greenbelt, MD 20771 USA.
[Tucker, Compton J.] NASA, Goddard Space Flight Ctr, Div Earth Sci, Greenbelt, MD 20771 USA.
RP Pinzon, JE (reprint author), NASA, Goddard Space Flight Ctr, Sci Syst & Applicat Inc, Biospher Sci Lab, Code 618, Greenbelt, MD 20771 USA.
EM jorge.e.pinzon@nasa.gov; compton.j.tucker@nasa.gov
FU NASA [NNH08CD31C]
FX This work was partially supported by NASA Applied Science grant
NNH08CD31C from 2009 to 2012. We thank the financial support by George
Collatz, Torry Johnson, and Molly Brown during the last year. We thank
Edwin Pak for processing the AVHRR/3 input data to NDVI3g.
Creating a consistent NDVI3g time series has been 8 years in
the making and many insightful works using the data set on their
analysis have contributed to its improvement. We thank supportive
feedback from George Collatz, Ranga Myneni, Uma Bhatt, Martha Raynolds,
Howard Epstein and Skip Walker and thank them for their comments on
various parts of this article. We also thank the anonymous reviewers for
their valuable remarks and suggestions. Lastly, two more important
acknowledgments: first, since digital data are ephemeral and access to
data involves infrastructure and economic support, we are in debt with
Ramakrishna Nemani and his group at NASA Earth Exchange (NEX) for
providing the infrastructure that supports data stewardship and makes it
viable. Second, we have been fortunate to interact with the group at the
SeaWiFS project. They not only provided us with high quality SeaWiFS
data, but also shared valuable information related to calibration, data
processing, and handling that is generally not included in scientific
journal articles.
NR 88
TC 112
Z9 118
U1 3
U2 42
PU MDPI AG
PI BASEL
PA ST ALBAN-ANLAGE 66, CH-4052 BASEL, SWITZERLAND
SN 2072-4292
J9 REMOTE SENS-BASEL
JI Remote Sens.
PD AUG
PY 2014
VL 6
IS 8
BP 6929
EP 6960
DI 10.3390/rs6086929
PG 32
WC Remote Sensing
SC Remote Sensing
GA AO7FV
UT WOS:000341518700008
ER
PT J
AU Lee, HJ
Zhang, SJ
Bar-Cohen, Y
Sherrit, S
AF Lee, Hyeong Jae
Zhang, Shujun
Bar-Cohen, Yoseph
Sherrit, Stewart
TI High Temperature, High Power Piezoelectric Composite Transducers
SO SENSORS
LA English
DT Review
DE piezocomposites; high temperature; high power; transducer; sensor
ID THERMAL-CONDUCTIVITY; ULTRASONIC TRANSDUCER; POLYMER COMPOSITES; PC-MUT;
CERAMICS; BIMORPHS; SENSOR; PIEZOCOMPOSITES; CONNECTIVITY; STABILITY
AB Piezoelectric composites are a class of functional materials consisting of piezoelectric active materials and non-piezoelectric passive polymers, mechanically attached together to form different connectivities. These composites have several advantages compared to conventional piezoelectric ceramics and polymers, including improved electromechanical properties, mechanical flexibility and the ability to tailor properties by using several different connectivity patterns. These advantages have led to the improvement of overall transducer performance, such as transducer sensitivity and bandwidth, resulting in rapid implementation of piezoelectric composites in medical imaging ultrasounds and other acoustic transducers. Recently, new piezoelectric composite transducers have been developed with optimized composite components that have improved thermal stability and mechanical quality factors, making them promising candidates for high temperature, high power transducer applications, such as therapeutic ultrasound, high power ultrasonic wirebonding, high temperature non-destructive testing, and downhole energy harvesting. This paper will present recent developments of piezoelectric composite technology for high temperature and high power applications. The concerns and limitations of using piezoelectric composites will also be discussed, and the expected future research directions will be outlined.
C1 [Lee, Hyeong Jae; Bar-Cohen, Yoseph; Sherrit, Stewart] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Lee, Hyeong Jae; Zhang, Shujun] Penn State Univ, Mat Res Inst, University Pk, PA 16802 USA.
RP Lee, HJ (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM hjlee@jpl.nasa.gov; soz1@psu.edu; yoseph.bar-cohen@jpl.nasa.gov;
stewart.sherrit@jpl.nasa.gov
FU ONR; NIH [2P41EB002182-15A1.O]
FX The authors thank to Thomas R. Shrout for the helpful discussions and
his supports. Some of the research reported in this manuscript was
conducted at the Jet Propulsion Laboratory (JPL), California Institute
of Technology, under a contract with National Aeronautics and Space
Administration (NASA). Also, part of the reported research was supported
by ONR and NIH under contract No. 2P41EB002182-15A1.O.
NR 96
TC 8
Z9 8
U1 11
U2 88
PU MDPI AG
PI BASEL
PA ST ALBAN-ANLAGE 66, CH-4052 BASEL, SWITZERLAND
SN 1424-8220
J9 SENSORS-BASEL
JI Sensors
PD AUG
PY 2014
VL 14
IS 8
BP 14526
EP 14552
DI 10.3390/s140814526
PG 27
WC Chemistry, Analytical; Electrochemistry; Instruments & Instrumentation
SC Chemistry; Electrochemistry; Instruments & Instrumentation
GA AO6YX
UT WOS:000341499900060
PM 25111242
ER
PT J
AU Han, XG
Funk, MR
Shen, F
Chen, YC
Li, YY
Campbell, CJ
Dai, JQ
Yang, XF
Kim, JW
Liao, YL
Connell, JW
Barone, V
Chen, ZF
Lin, Y
Hu, LB
AF Han, Xiaogang
Funk, Michael R.
Shen, Fei
Chen, Yu-Chen
Li, Yuanyuan
Campbell, Caroline J.
Dai, Jiaqi
Yang, Xiaofeng
Kim, Jae-Woo
Liao, Yunlong
Connell, John W.
Barone, Veronica
Chen, Zhongfang
Lin, Yi
Hu, Liangbing
TI Scalable Holey Graphene Synthesis and Dense Electrode Fabrication toward
High-Performance Ultracapacitors
SO ACS NANO
LA English
DT Article
DE scalable synthesis; facile processability; holey graphene; dense
graphene electrode; ultracapacitor; supercapacitor; volumetric
capacitance
ID SCANNING-TUNNELING-MICROSCOPY; ORIENTED PYROLYTIC-GRAPHITE; ACTIVATED
GRAPHENE; ENERGY-STORAGE; SUPERCAPACITOR ELECTRODES;
MOLECULAR-MECHANICS; OXIDE; FILMS; OXIDATION; NANOMESH
AB Graphene has attracted a lot of attention for ultracapacitor electrodes because of its high electrical conductivity, high surface area and superb chemical stability. However, poor volumetric capacitive performance of typical graphene-based electrodes has hindered their practical applications because of the extremely low density. Herein we report a scalable synthesis method of holey graphene (h-Graphene) in a single step without using any catalysts or special chemicals The film made of the as synthesized h-Graphene exhibited relatively strong mechanical strength, 2D hole morphology, high density, and facile processability. This scalable one-step synthesis method for h-Graphene is time environmentally friendly, and generally applicable to other two-dimensional materials The ultracapacitor electrodes based on remarkably improved volumetric capacitance with about 700% increase compared to that of regular graphene electrodes. h-Graphene was carried out to understand the excellent processability and improved ultracapacitor performance. efficient, the h-Graphene show a Modeling on individual cost-efficient,
C1 [Han, Xiaogang; Shen, Fei; Chen, Yu-Chen; Li, Yuanyuan; Dai, Jiaqi; Yang, Xiaofeng; Hu, Liangbing] Univ Maryland, Dept Mat Sci & Engn, College Pk, MD 20742 USA.
[Funk, Michael R.; Lin, Yi] Coll William & Mary, Dept Appl Sci, Williamsburg, VA 23185 USA.
[Funk, Michael R.; Connell, John W.] NASA, Adv Mat & Proc Branch, Langley Res Ctr, Hampton, VA 23681 USA.
[Campbell, Caroline J.; Kim, Jae-Woo; Liao, Yunlong; Lin, Yi] Natl Inst Aerosp, Hampton, VA 23666 USA.
[Barone, Veronica] Cent Michigan Univ, Adv Mat Program, Dept Phys & Sci, Mt Pleasant, MI 48859 USA.
[Liao, Yunlong; Chen, Zhongfang] Univ Puerto Rico, Inst Funct Nanomat, Dept Chem, San Juan, PR 00931 USA.
RP Lin, Y (reprint author), Coll William & Mary, Dept Appl Sci, Williamsburg, VA 23185 USA.
EM yi.lin@nianet.org; binghu@umd.edu
RI Kim, Jae-Woo/A-8314-2008; Barone, Veronica/C-2634-2008; Chen,
Zhongfang/A-3397-2008; Hu, Liangbing/N-6660-2013; Han,
Xiaogang/D-6430-2015
OI Han, Xiaogang/0000-0002-4785-6506
FU NSF-CBET [1335944, 1335979]; Leading Edge Aeronautics Research for NASA
(LEARN) program [NNX13AB88A]; NASA Pathways Intern Employment Program
(IEP); LEARN; Department of Defense [W911NF-12-1-0083]; NASA
[NNX10AM80H, NNX13AB22A]
FX The authors thank Dr. W. Cao and Prof. H. Elsayed-Ali at Applied
Research Center of Old Dominion University for their experimental
assistance in acquiring TEM images. V.B. and L.H. gratefully acknowledge
the support from NSF-CBET Grant Nos. 1335944 and 1335979, respectively.
Y.L. and J.K. acknowledge the financial support from the Leading Edge
Aeronautics Research for NASA (LEARN) program (Grant No. NNX13AB88A).
M.F. is supported by the NASA Pathways Intern Employment Program (IEP).
C.C. was a Langley Aerospace Research Summer Scholars (LARSS) Program
scholar supported by LEARN. Z.C. acknowledges the support by Department
of Defense (Grant No. W911NF-12-1-0083) and NASA (Grant Nos. NNX10AM80H
and NNX13AB22A). We thank Prof. D. DeVoe, Dr. E. Kendall, and the
Maryland Microfluidic Laboratory (MML) for providing access to the
goniometer.
NR 45
TC 50
Z9 50
U1 32
U2 246
PU AMER CHEMICAL SOC
PI WASHINGTON
PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA
SN 1936-0851
EI 1936-086X
J9 ACS NANO
JI ACS Nano
PD AUG
PY 2014
VL 8
IS 8
BP 8255
EP 8265
DI 10.1021/nn502635y
PG 11
WC Chemistry, Multidisciplinary; Chemistry, Physical; Nanoscience &
Nanotechnology; Materials Science, Multidisciplinary
SC Chemistry; Science & Technology - Other Topics; Materials Science
GA AO0IM
UT WOS:000340992300072
PM 25093751
ER
PT J
AU Bishop, JL
Quinn, R
Dyar, MD
AF Bishop, Janice L.
Quinn, Richard
Dyar, M. Darby
TI Spectral and thermal properties of perchlorate salts and implications
for Mars
SO AMERICAN MINERALOGIST
LA English
DT Article
DE Perchlorate; Mars; reflectance spectroscopy; differential scanning
calorimetry; hydrated salts
ID CRYSTAL-STRUCTURE; INFRARED-SPECTRA; EMISSION-SPECTROSCOPY; SOUTHERN
HIGHLANDS; RAMAN-SPECTROSCOPY; PHASE-TRANSITIONS; MARTIAN SOIL; LANDING
SITE; COMPLEXES; CHEMISTRY
AB K+, Na2+, Mg2+, Fe2+, Fe3+, and Al3+ perchlorate salts were studied to provide spectral and thermal data for detecting and characterizing their possible presence on Mars. Spectral and thermal analyses are coordinated with structural analyses to understand how different cations and different hydration levels affect the mineral system. Near-infrared (NIR) spectral features for perchlorates are dominated by H2O bands that occur at 0.978-1.01, 1.17-1.19, 1.42-1.48, 1.93-1.99, and 2.40-2.45 mu m. Mid-IR spectral features are observed for vibrations of the tetrahedral ClO4- ion and occur as reflectance peaks at 1105-1130 cm(-1) (similar to 8.6-9 mu m), 760-825 cm(-1) (similar to 12-13 mu m), 630 cm(-1) (similar to 15.9 mu m), 460-495 (similar to 20-22 pm), and 130-215 (similar to 50-75 mu m). The spectral bands in both regions are sensitive to the type of cation present because the polarizing power is related to the band center for many of the spectral features. Band assignments were confirmed for many of the spectral features due to opposing trends in vibrational energies for the ClO4-, and H2O groups connected to different octahedral cations. Differential scanning calorimetry (DSC) data show variable patterns of water loss and thermal decomposition temperatures for perchlorates with different cations, consistent with changes in spectral features measured under varying hydration conditions. Results of the DSC analyses indicate that the bond energies of H2O in perchlorates are different for each cation and hydration state. Structural parameters are available for Mg perchlorates (Robertson and Bish 2010) and the changes in structure due to hydration state are consistent with DSC parameters and spectral features. Analyses of changes in the Mg perchlorate structures with H2O content inform our understanding of the effects of hydration on other perchlorates, for which the specific structures are less well defined. Spectra of the hydrated Fe2+ and Fe3+ perchlorates changed significantly upon heating to 100 degrees C or measurement under low-moisture conditions indicating that they are less stable than other perchlorates under dehydrated conditions. The perchlorate abundances observed by Phoenix and MSL are likely too low to be identified from orbit by CRISM, but may be sufficient to be identifiable by a VNIR imager on a future rover.
C1 [Bishop, Janice L.; Quinn, Richard] Carl Sagan Ctr, SETI Inst, Mountain View, CA 94043 USA.
[Bishop, Janice L.; Quinn, Richard] NASA, Ames Res Ctr, Space Sci & Astrobiol Div, Moffett Field, CA 94035 USA.
[Dyar, M. Darby] Mt Holyoke Coll, Dept Astron, S Hadley, MA 01075 USA.
RP Bishop, JL (reprint author), Carl Sagan Ctr, SETI Inst, Mountain View, CA 94043 USA.
EM jbishop@seti.org
FU NASA Astrobiology: Exobiology and Evolutionary Biology Program
[NNX09AM93G, NNX13A167G]
FX We are grateful for support from NASA Astrobiology: Exobiology and
Evolutionary Biology Program grants NNX09AM93G and NNX13A167G. We also
thank T. Hiroi at Brown University's RELAB for measuring many of the
reflectance spectra used in the study and the helpful suggestions from
two anonymous reviewers.
NR 87
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Z9 7
U1 3
U2 29
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 AUG-SEP
PY 2014
VL 99
IS 8-9
BP 1580
EP 1592
DI 10.2138/am.2014.4707
PG 13
WC Geochemistry & Geophysics; Mineralogy
SC Geochemistry & Geophysics; Mineralogy
GA AN4TD
UT WOS:000340580500008
ER
PT J
AU Pitman, KM
Dobrea, EZN
Jamieson, CS
Dalton, JB
Abbey, WJ
Joseph, ECS
AF Pitman, Karly M.
Dobrea, Eldar Z. Noe
Jamieson, Corey S.
Dalton, James B., III
Abbey, William J.
Joseph, Emily C. S.
TI Reflectance spectroscopy and optical functions for hydrated Fe-sulfates
SO AMERICAN MINERALOGIST
LA English
DT Article
DE Jarosite; szomolnokite; rhomboclase; optical constants; visible to
near-infrared wavelength; laboratory diffuse reflectance spectroscopy
ID THERMAL EMISSION-SPECTRA; SOLID-SOLUTION SERIES; PARTICULATE SURFACES;
MARTIAN METEORITES; CRYSTAL-CHEMISTRY; NAKHLA METEORITE; SITE OCCUPANCY;
MARS; MINERALS; JAROSITE
AB Visible and near-infrared wavelength (VNIR, lambda = 0.35-5 mu m) laboratory diffuse reflectance spectra and corresponding optical functions (real and imaginary refractive indices) for several iron sulfates (natural K- and Na-jarosite, szomolnokite, rhomboclase) are presented. On Mars, jarosite has been identified in Meridiani Planum, Mawrth Vallis, Melas Chasma, and Eridania Basin; szomolnokite has been found as distinct layers at Columbus Crater and as outcrops at Juventae Chasma, and rhomboclase has been identified at Gusev Crater. Constraining the mineralogy and chemistry (Fe- vs. Mg-rich) of the sulfates on Mars may contribute to our understanding of the environmental and aqueous conditions present on Mars during their formation. The data presented here will help to constrain the mineralogy, abundance, and distribution of sulfates on the martian surface, which will lead to improvements in understanding the pressure, temperature, and humidity conditions and how active frost, groundwater, and atmospheric processes once were on Mars.
C1 [Pitman, Karly M.; Dobrea, Eldar Z. Noe; Joseph, Emily C. S.] Planetary Sci Inst, Tucson, AZ 85719 USA.
[Jamieson, Corey S.] SETI Inst, Mountain View, CA 94043 USA.
[Dalton, James B., III; Abbey, William J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Pitman, KM (reprint author), Planetary Sci Inst, 1700 E Ft Lowell Rd,Suite 106, Tucson, AZ 85719 USA.
EM pitman@psi.edu
FU NASA's Mars Fundamental Research Program [NNX10AP78G]
FX This work was supported by NASA's Mars Fundamental Research Program
(NNX10AP78G: PI Pitman) and partly performed at the Jet Propulsion
Laboratory, California Institute of Technology, under contract to the
National Aeronautics and Space Administration. The authors thank Robert
Anderson, Janice Bishop, Adrian Brown, Ed Cloutis, Ken Farley, Troy
Hudson, Joel Hurowitz, Brendt Hyde, Penny King, and Melissa Lane for
helpful comments, conversations, and assistance with samples and
equipment. This is PSI Contribution No. 614.
NR 84
TC 3
Z9 3
U1 1
U2 17
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 AUG-SEP
PY 2014
VL 99
IS 8-9
BP 1593
EP 1603
DI 10.2138/am.2014.4730
PG 11
WC Geochemistry & Geophysics; Mineralogy
SC Geochemistry & Geophysics; Mineralogy
GA AN4TD
UT WOS:000340580500009
ER
PT J
AU Werdell, PJ
Roesler, CS
Goes, JI
AF Werdell, P. Jeremy
Roesler, Collin S.
Goes, Joaquim I.
TI Discrimination of phytoplankton functional groups using an ocean
reflectance inversion model
SO APPLIED OPTICS
LA English
DT Article
ID INHERENT OPTICAL-PROPERTIES; CHLOROPHYLL-A CONCENTRATION;
ABSORPTION-COEFFICIENTS; BACKSCATTERING RATIO; COLOR RADIOMETRY;
LIGHT-ABSORPTION; CHESAPEAKE BAY; CASE-1 WATERS; SIZE CLASSES; ARABIAN
SEA
AB Ocean reflectance inversion models (ORMs) provide a mechanism for inverting the color of the water observed by a satellite into marine inherent optical properties (IOPs), which can then be used to study phytoplankton community structure. Most ORMs effectively separate the total signal of the collective phytoplankton community from other water column constituents; however, few have been shown to effectively identify individual contributions by multiple phytoplankton groups over a large range of environmental conditions. We evaluated the ability of an ORM to discriminate between Noctiluca miliaris and diatoms under conditions typical of the northern Arabian Sea. We: (1) synthesized profiles of IOPs that represent bio-optical conditions for the Arabian Sea; (2) generated remote-sensing reflectances from these profiles using Hydrolight; and (3) applied the ORM to the synthesized reflectances to estimate the relative concentrations of diatoms and N. miliaris. By comparing the estimates from the inversion model with those from synthesized vertical profiles, we identified those conditions under which the ORM performs both well and poorly. Even under perfectly controlled conditions, the absolute accuracy of ORM retrievals degraded when further deconstructing the derived total phytoplankton signal into subcomponents. Although the absolute magnitudes maintained biases, the ORM successfully detected whether or not Noctiluca miliaris appeared in the simulated water column. This quantitatively calls for caution when interpreting the absolute magnitudes of the retrievals, but qualitatively suggests that the ORM provides a robust mechanism for identifying the presence or absence of species. (C) 2014 Optical Society of America
C1 [Werdell, P. Jeremy] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Werdell, P. Jeremy] Univ Maine, Sch Marine Sci, Orono, ME 04469 USA.
[Roesler, Collin S.] Bowdoin Coll, Dept Earth & Ocean Sci, Brunswick, ME 04011 USA.
[Goes, Joaquim I.] Columbia Univ, Lamont Doherty Earth Observ, Palisades, NY 10964 USA.
RP Werdell, PJ (reprint author), NASA, Goddard Space Flight Ctr, Code 616, Greenbelt, MD 20771 USA.
EM jeremy.werdell@nasa.gov
FU NASA Ocean Biology and Biogeochemistry Program [NNX11AE22G]
FX Many thanks to Sean Bailey, Gene Feldman, Curt Mobley, Mary Jane Perry,
Andrew Thomas, Huijie Xue, and Emmanuel Boss for their advice throughout
the development of this manuscript. Thanks also to Susan Drapeau, Kelly
Keebler, Helga do Rosario Gomes, Prahbu Matondkar, and colleagues at the
National Institute of Oceanography, India for their support with field
experiments and data analysis. Finally, many thanks to Stephane
Maritorena and an anonymous reviewer for their exceptional comments and
attention to detail. Support for this work was provided through the NASA
Ocean Biology and Biogeochemistry Program under research grant
NNX11AE22G.
NR 74
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Z9 7
U1 4
U2 20
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 AUG 1
PY 2014
VL 53
IS 22
BP 4833
EP 4849
DI 10.1364/AO.53.004833
PG 17
WC Optics
SC Optics
GA AN8BC
UT WOS:000340824800017
PM 25090312
ER
PT J
AU Roberts, LE
Ward, RL
Sutton, AJ
Fleddermann, R
de Vine, G
Malikides, EA
Wuchenich, DMR
McClelland, DE
Shaddock, DA
AF Roberts, Lyle E.
Ward, Robert L.
Sutton, Andrew J.
Fleddermann, Roland
de Vine, Glenn
Malikides, Emmanuel A.
Wuchenich, Danielle M. R.
McClelland, David E.
Shaddock, Daniel A.
TI Coherent beam combining using a 2D internally sensed optical phased
array
SO APPLIED OPTICS
LA English
DT Article
ID ENHANCED HETERODYNE INTERFEROMETRY; FIBER AMPLIFIER; KW; LOCKING
AB Coherent combination of multiple lasers using an optical phased array (OPA) is an effective way to scale optical intensity in the far field beyond the capabilities of single fiber lasers. Using an actively phase locked, internally sensed, 2D OPA we demonstrate over 95% fringe visibility of the interfered beam, lambda/120 RMS output phase stability over a 5 Hz bandwidth, and quadratic scaling of intensity in the far field using three emitters. This paper presents a new internally sensed OPA architecture that employs a modified version of digitally enhanced heterodyne interferometry (DEHI) based on code division multiplexing to measure and control the phase of each emitter. This internally sensed architecture can be implemented with no freespace components, offering improved robustness to shock and vibration exhibited by all-fiber devices. To demonstrate the concept, a single laser is split into three channels/emitters, each independently controlled using separate electro-optic modulators. The output phase of each channel is measured using DEHI to sense the small fraction of light that is reflected back into the fiber at the OPA's glass-air interface. The relative phase between emitters is used to derive the control signals needed to stabilize their relative path lengths and maintain coherent combination in the far field. (C) 2014 Optical Society of America
C1 [Roberts, Lyle E.; Ward, Robert L.; Sutton, Andrew J.; Fleddermann, Roland; Malikides, Emmanuel A.; Wuchenich, Danielle M. R.; McClelland, David E.; Shaddock, Daniel A.] Australian Natl Univ, Dept Quantum Sci, Canberra, ACT 0200, Australia.
[de Vine, Glenn] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Roberts, LE (reprint author), Australian Natl Univ, Dept Quantum Sci, GPO Box 4, Canberra, ACT 0200, Australia.
EM Lyle.Roberts@anu.edu.au
RI McClelland, David/E-6765-2010; Shaddock, Daniel/A-7534-2011; Ward,
Robert/I-8032-2014
OI McClelland, David/0000-0001-6210-5842; Shaddock,
Daniel/0000-0002-6885-3494; Ward, Robert/0000-0001-5503-5241
NR 11
TC 1
Z9 1
U1 3
U2 12
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 AUG 1
PY 2014
VL 53
IS 22
BP 4881
EP 4885
DI 10.1364/AO.53.004881
PG 5
WC Optics
SC Optics
GA AN8BC
UT WOS:000340824800022
PM 25090317
ER
PT J
AU Potter, C
AF Potter, Christopher
TI Regional analysis of MODIS satellite greenness trends for ecosystems of
interior Alaska
SO GISCIENCE & REMOTE SENSING
LA English
DT Article
DE MODIS EVI; forest; tundra; wetlands; wildfire; Alaska
ID POSTFIRE VEGETATION; FIRE DISTURBANCE; FOREST RECOVERY; BURN SEVERITY;
TIME-SERIES; CLIMATE; VULNERABILITY; INDEXES; GROWTH; TUNDRA
AB Trends in the growing season Moderate Resolution Imaging Spectroradiometer (MODIS) Enhanced Vegetation Index (EVI) time-series were analyzed for the time period from 2000 to 2010 to understand landscape-level patterns of vegetation change in ecosystems of interior Alaska. The analysis compared data-sets for Alaska vegetation cover types, wetland cover classes, wildfire boundaries since the 1940s, permafrost type, and elevation to identify the most likely combination of factors driving regional changes in habitat quality and ecosystem productivity. Approximately 48% of all ecosystem areas in interior Alaska were detected with significant (p < 0.05) positive or negative MODIS growing season EVI trends from 2000 to 2010. Three-quarters of these ecosystem areas (nearly 110,000 km(2)) were detected with significant positive growing season EVI trends. The vast majority of interior Alaska area detected with significant positive growing season EVI trends was classified as upland shrub cover, although non-forested wetlands (marshes, bogs, fens, and floodplains) were colocated on 13% of that total area. Evidence supports the hypothesis that temperature (warming) has markedly enhanced the rates of shrubland and tundra vegetation growth across interior Alaska over recent years.
C1 NASA, Ames Res Ctr, Mountain View, CA 94035 USA.
RP Potter, C (reprint author), NASA, Ames Res Ctr, Mail Stop 232-21, Mountain View, CA 94035 USA.
EM chris.potter@nasa.gov
FU NASA under the US National Climate Assessment
FX This work was conducted with support from NASA under the US National
Climate Assessment.
NR 33
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U1 4
U2 21
PU TAYLOR & FRANCIS LTD
PI ABINGDON
PA 4 PARK SQUARE, MILTON PARK, ABINGDON OX14 4RN, OXON, ENGLAND
SN 1548-1603
EI 1943-7226
J9 GISCI REMOTE SENS
JI GISci. Remote Sens.
PD AUG
PY 2014
VL 51
IS 4
BP 390
EP 402
DI 10.1080/15481603.2014.933606
PG 13
WC Geography, Physical; Remote Sensing
SC Physical Geography; Remote Sensing
GA AN9TG
UT WOS:000340951100003
ER
PT J
AU Kereszturi, A
Blumberger, Z
Jozsa, S
May, Z
Muller, A
Szabo, M
Toth, M
AF Kereszturi, A.
Blumberger, Z.
Jozsa, S.
May, Z.
Mueller, A.
Szabo, M.
Toth, M.
TI Alteration processes in the CV chondrite parent body based on analysis
of NWA 2086 meteorite
SO METEORITICS & PLANETARY SCIENCE
LA English
DT Article
ID CARBONACEOUS CHONDRITE; AQUEOUS ALTERATION; MINERAL CHEMISTRY; ALLENDE
METEORITE; CM CHONDRITES; SOLAR NEBULA; DARK RIMS; ORIGIN; INCLUSIONS;
CHONDRULES
AB Analysis of the NWA 2086 CV3 chondrite showed a matrix/chondrule ratio of 52%, similar to Bali, Mokoia, and Grosanaja. Nearly twice as many chondrule fragments as intact ones demonstrate that an early fragmentation phase occurred prior to final accretion. After this event, no substantial mechanical change or redeposition is evident. Rims with double-layered structures were identified around some chondrules, which, in at least one case, is attributed to an accretionary origin. The rim's outer parts with a diffuse appearance were formed by in situ chemical alteration. During this later process, Mg content decreased, Fe content increased, and olivine composition was homogenized, producing a rim composition close to that of the matrix. This alteration occasionally happened along fractures and at confined locations, and was probably produced by fluid interactions. Iron oxides are the best candidate for a small grain-sized alteration product; however, technical limitations in the available equipment did not allow exact phase identification. These results suggest that NWA 2086 came from a location (possible more deeply buried) in the CV parent body than Mokoia or Bali, and suffered less impact effects-although there is no evidence of sustained thermal alteration. This meteorite may represent a sample of the CV parent asteroid interior and provide a useful basis for comparison with other CV meteorites in the future.
C1 [Kereszturi, A.] Hungarian Acad Sci, Res Ctr Astron & Earth Sci, Konkoly Thege Miklos Astron Inst, Astrophys & Geochem Lab, H-1121 Budapest, Hungary.
[Blumberger, Z.] Eotvos Lorand Univ Sci, Hungarian Acad Sci, Fac Sci, Ctr Environm Sci, H-1117 Budapest, Hungary.
[Jozsa, S.] Eotvos Lorand Univ Sci, Dept Petr & Geochem, Fac Sci, Hungarian Acad Sci, H-1117 Budapest, Hungary.
[May, Z.] Hungarian Acad Sci, Chem Res Ctr, Inst Mat & Environm Chem, H-1025 Budapest, Hungary.
[Mueller, A.; Szabo, M.; Toth, M.] Hungarian Acad Sci, Inst Geol & Geochem Res, Res Ctr Astron & Earth Sci, H-1112 Budapest, Hungary.
[Kereszturi, A.] NASA, Astrobiol Inst, Thermodynam Disequilibrium & Evolut Focus Grp, Washington, DC USA.
RP Kereszturi, A (reprint author), Hungarian Acad Sci, Res Ctr Astron & Earth Sci, Konkoly Thege Miklos Astron Inst, Astrophys & Geochem Lab, Konkoly 15-17, H-1121 Budapest, Hungary.
EM kereszturi.akos@csfk.mta.hu
FU Astrophysical and Geochemical Laboratory of CSFK, Hungary; Hungarian
Academy of Sciences; COST [TD1308, TET_12_FR-1-2013-0023]
FX This work was supported by the Astrophysical and Geochemical Laboratory
of CSFK, Hungary, and also the Infrastructure and other related CSFK
Fund of the Hungarian Academy of Sciences. The COST TD1308 and
TET_12_FR-1-2013-0023 projects are also acknowledged. The authors thank
the helpful suggestions from referees: M. Zolenksy, K. Fintor, an
anonymous reviewer, and the editor T. Jull.
NR 59
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PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 1086-9379
EI 1945-5100
J9 METEORIT PLANET SCI
JI Meteorit. Planet. Sci.
PD AUG
PY 2014
VL 49
IS 8
BP 1350
EP 1364
DI 10.1111/maps.12336
PG 15
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA AN8SZ
UT WOS:000340875900004
ER
PT J
AU Jenniskens, P
Rubin, AE
Yin, QZ
Sears, DWG
Sandford, SA
Zolensky, ME
Krot, AN
Blair, L
Kane, D
Utas, J
Verish, R
Friedrich, JM
Wimpenny, J
Eppich, GR
Ziegler, K
Verosub, KL
Rowland, DJ
Albers, J
Gural, PS
Grigsby, B
Fries, MD
Matson, R
Johnston, M
Silber, E
Brown, P
Yamakawa, A
Sanborn, ME
Laubenstein, M
Welten, KC
Nishiizumi, K
Meier, MMM
Busemann, H
Clay, P
Caffee, MW
Schmitt-Kopplin, P
Hertkorn, N
Glavin, DP
Callahan, MP
Dworkin, JP
Wu, QH
Zare, RN
Grady, M
Verchovsky, S
Emel'yanenko, V
Naroenkov, S
Clark, DL
Girten, B
Worden, PS
AF Jenniskens, Peter
Rubin, Alan E.
Yin, Qing-Zhu
Sears, Derek W. G.
Sandford, Scott A.
Zolensky, Michael E.
Krot, Alexander N.
Blair, Leigh
Kane, Darci
Utas, Jason
Verish, Robert
Friedrich, Jon M.
Wimpenny, Josh
Eppich, Gary R.
Ziegler, Karen
Verosub, Kenneth L.
Rowland, Douglas J.
Albers, Jim
Gural, Peter S.
Grigsby, Bryant
Fries, Marc D.
Matson, Robert
Johnston, Malcolm
Silber, Elizabeth
Brown, Peter
Yamakawa, Akane
Sanborn, Matthew E.
Laubenstein, Matthias
Welten, Kees C.
Nishiizumi, Kunihiko
Meier, Matthias M. M.
Busemann, Henner
Clay, Patricia
Caffee, Marc W.
Schmitt-Kopplin, Phillipe
Hertkorn, Norbert
Glavin, Daniel P.
Callahan, Michael P.
Dworkin, Jason P.
Wu, Qinghao
Zare, Richard N.
Grady, Monica
Verchovsky, Sasha
Emel'yanenko, Vacheslav
Naroenkov, Sergey
Clark, David L.
Girten, Beverly
Worden, Peter S.
CA Novato Meteorite Consortium
TI Fall, recovery, and characterization of the Novato L6 chondrite breccia
SO METEORITICS & PLANETARY SCIENCE
LA English
DT Article
ID UNEQUILIBRATED ORDINARY CHONDRITES; PARK-FOREST METEORITE; INNER
SOLAR-SYSTEM; COSMOGENIC NUCLIDES; EXPOSURE HISTORY; OXYGEN-ISOTOPE;
CARBONACEOUS CHONDRITES; INNISFREE METEORITE; ASTEROIDAL SOURCE; STONY
METEORITES
AB The Novato L6 chondrite fragmental breccia fell in California on 17 October 2012, and was recovered after the Cameras for Allsky Meteor Surveillance (CAMS) project determined the meteor's trajectory between 95 and 46 km altitude. The final fragmentation from 42 to 22 km altitude was exceptionally well documented by digital photographs. The first sample was recovered before rain hit the area. First results from a consortium study of the meteorite's characterization, cosmogenic and radiogenic nuclides, origin, and conditions of the fall are presented. Some meteorites did not retain fusion crust and show evidence of spallation. Before entry, the meteoroid was 35 +/- 5 cm in diameter (mass 80 +/- 35 kg) with a cosmic-ray exposure age of 9 +/- 1 Ma, if it had a one-stage exposure history. A two-stage exposure history is more likely, with lower shielding in the last few Ma. Thermoluminescence data suggest a collision event within the last similar to 0.1 Ma. Novato probably belonged to the class of shocked L chondrites that have a common shock age of 470 Ma, based on the U, Th-He age of 420 +/- 220 Ma. The measured orbits of Novato, Jesenice, and Innisfree are consistent with a proposed origin of these shocked L chondrites in the Gefion asteroid family, perhaps directly via the 5: 2 mean-motion resonance with Jupiter. Novato experienced a stronger compaction than did other L6 chondrites of shock-stage S4. Despite this, a freshly broken surface shows a wide range of organic compounds.
C1 [Jenniskens, Peter; Blair, Leigh; Albers, Jim; Gural, Peter S.; Grigsby, Bryant] Carl Sagan Ctr, SETI Inst, Mountain View, CA 94043 USA.
[Jenniskens, Peter; Sears, Derek W. G.; Sandford, Scott A.; Girten, Beverly; Worden, Peter S.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Rubin, Alan E.] Univ Calif Los Angeles, Inst Geophys & Planetary Phys, Los Angeles, CA 90095 USA.
[Yin, Qing-Zhu; Wimpenny, Josh; Verosub, Kenneth L.; Yamakawa, Akane; Sanborn, Matthew E.] Univ Calif Davis, Dept Earth & Planetary Sci, Davis, CA 95616 USA.
[Sears, Derek W. G.] BAER Inst, Mountain View, CA 94043 USA.
[Zolensky, Michael E.; Fries, Marc D.] NASA, Johnson Space Ctr, Houston, TX 77801 USA.
[Krot, Alexander N.] Univ Hawaii Manoa, Hawaii Inst Geophys & Planetol, Honolulu, HI 96822 USA.
[Kane, Darci] Buck Inst, Novato, CA 94945 USA.
[Utas, Jason] Univ Calif Los Angeles, Inst Geophys & Planetary Phys, Los Angeles, CA 90095 USA.
[Verish, Robert] Meteorite Recovery Lab, Escondido, CA 92046 USA.
[Friedrich, Jon M.] Fordham Univ, Dept Chem, Bronx, NY 10458 USA.
[Friedrich, Jon M.] Amer Museum Nat Hist, Dept Earth & Planetary Sci, New York, NY 10024 USA.
[Eppich, Gary R.] Lawrence Livermore Natl Lab, Glenn Seaborg Inst, Livermore, CA 94550 USA.
[Ziegler, Karen] Univ New Mexico, Inst Meteorit, Albuquerque, NM 87131 USA.
[Rowland, Douglas J.] Univ Calif Davis, Ctr Mol & Genom Imaging, Davis, CA 95616 USA.
[Matson, Robert] SAIC, San Diego, CA 92121 USA.
[Johnston, Malcolm] US Geol Survey, Menlo Pk, CA 94025 USA.
[Silber, Elizabeth; Brown, Peter; Clark, David L.] Univ Western Ontario, Dept Phys & Astron, London, ON N6A 3K7, Canada.
[Laubenstein, Matthias] Inst Nazl Fis Nucl, Lab Nazl Gran Sasso, I-67010 Assergi, AQ, Italy.
[Welten, Kees C.; Nishiizumi, Kunihiko] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
[Meier, Matthias M. M.] ETH, Dept Earth Sci, CH-8092 Zurich, Switzerland.
[Meier, Matthias M. M.] Lund Univ, Dept Geol, SE-22362 Lund, Sweden.
[Busemann, Henner; Clay, Patricia] Univ Manchester, SEAES, Manchester M13 9PL, Lancs, England.
[Caffee, Marc W.] Purdue Univ, Dept Phys, W Lafayette, IN 47907 USA.
[Schmitt-Kopplin, Phillipe; Hertkorn, Norbert] Helmholtz Zentrum Munchen, BGC, D-85764 Munich, Germany.
[Schmitt-Kopplin, Phillipe] Tech Univ Munich, ALC, D-85354 Freising Weihenstephan, Germany.
[Glavin, Daniel P.; Callahan, Michael P.; Dworkin, Jason P.] NASA, Goddard Space Flight Ctr, Solar Syst Explorat Div, Greenbelt, MD 20771 USA.
[Wu, Qinghao; Zare, Richard N.] Stanford Univ, Dept Chem, Stanford, CA 94305 USA.
[Grady, Monica; Verchovsky, Sasha] Open Univ, Planetary & Space Sci Res Inst, Milton Keynes MK7 6AA, Bucks, England.
[Emel'yanenko, Vacheslav; Naroenkov, Sergey] Russian Acad Sci INASAN, Inst Astron, Moscow 119017, Russia.
RP Jenniskens, P (reprint author), Carl Sagan Ctr, SETI Inst, Mountain View, CA 94043 USA.
EM petrus.m.jenniskens@nasa.gov
RI Naroenkov, Sergey/I-5699-2013; Emel'yanenko, Vacheslav/A-4087-2014; Yin,
Qing-Zhu/B-8198-2009; Caffee, Marc/K-7025-2015; Laubenstein,
Matthias/C-4851-2013; Glavin, Daniel/D-6194-2012; Schmitt-Kopplin,
Philippe/H-6271-2011; Dworkin, Jason/C-9417-2012;
OI Eppich, Gary/0000-0003-2176-6673; Yin, Qing-Zhu/0000-0002-4445-5096;
Caffee, Marc/0000-0002-6846-8967; Grady, Monica/0000-0002-4055-533X;
Laubenstein, Matthias/0000-0001-5390-4343; Glavin,
Daniel/0000-0001-7779-7765; Schmitt-Kopplin,
Philippe/0000-0003-0824-2664; Dworkin, Jason/0000-0002-3961-8997;
Busemann, Henner/0000-0002-0867-6908; Meier,
Matthias/0000-0002-7179-4173; Rowland, Douglas/0000-0001-8059-6905;
Clark, David/0000-0002-1203-764X; Sanborn, Matthew/0000-0003-3218-1195
FU NASA [NNX12AM14G, NNX08AO64G]; NASA Cosmochemistry program [NNG06GF95G,
NNX11AJ51G, NNX11AC69G]; Swiss National Science Foundation (STFC)
FX This consortium study was made possible thanks to the donation of
meteorite N01 by Novato residents Lisa Webber and Glenn Rivera. Lynn
Hofland of NASA Ames Research Center performed the tensile strength
measurements. This work was supported by the NASA Near Earth Object
Observation and Planetary Astronomy programs (NNX12AM14G and NNX08AO64G
to P.J.), the NASA Cosmochemistry program (NNG06GF95G to A. R.,
NNX11AJ51G to Q.Z.Y. & A.N.K., and NNX11AC69G to K.N.), and the Swiss
National Science Foundation (STFC).
NR 124
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U1 0
U2 17
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 1086-9379
EI 1945-5100
J9 METEORIT PLANET SCI
JI Meteorit. Planet. Sci.
PD AUG
PY 2014
VL 49
IS 8
BP 1388
EP 1425
DI 10.1111/maps.12323
PG 38
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA AN8SZ
UT WOS:000340875900007
ER
PT J
AU Yin, QZ
Zhou, Q
Li, QL
Li, XH
Liu, Y
Tang, GQ
Krot, AN
Jenniskens, P
AF Yin, Qing-Zhu
Zhou, Qin
Li, Qiu-Li
Li, Xian-Hua
Liu, Yu
Tang, Guo-Qiang
Krot, Alexander N.
Jenniskens, Peter
TI Records of the Moon-forming impact and the 470 Ma disruption of the L
chondrite parent body in the asteroid belt from U-Pb apatite ages of
Novato (L6)
SO METEORITICS & PLANETARY SCIENCE
LA English
DT Article
ID ORDOVICIAN BIODIVERSIFICATION; FOSSIL METEORITES; SHOCK; CHROMITE; LEAD;
OXYGEN; ORIGIN; EARTH; METAMORPHISM; AR-40-AR-39
AB Novato, a newly observed fall in the San Francisco Bay area, is a shocked and brecciated L6 ordinary chondrite containing dark and light lithologies. We have investigated the U-Pb isotope systematics of coarse Cl-apatite grains of metamorphic origin in Novato with a large geometry ion microprobe. The U-Pb systematics of Novato apatite reveals an upper intercept age of 4472 +/- 31 Ma and lower intercept age of 473 +/- 38 Ma. The upper intercept age is within error identical to the U-Pb apatite age of 4452 +/- 21 Ma measured in the Chelyabinsk LL5 chondrite. This age is interpreted to reflect a massive collisional resetting event due to a large impact associated with the peak arrival time at the primordial asteroid belt of ejecta debris from the Moon-forming giant impact on Earth. The lower intercept age is consistent with the most precisely dated Ar-Ar ages of 470 +/- 6 Ma of shocked L chondrites, and the fossil meteorites and extraterrestrial chromite relicts found in Ordovician limestones with an age of 467.3 +/- 1.6 Ma in Sweden and China. The lower intercept age reflects a major disturbance related to the catastrophic disruption of the L chondrite parent body most likely associated with the Gefion asteroid family, which produced an initially intense meteorite bombardment of the Earth in Ordovician period and reset and degassed at least approximately 35% of the L chondrite falls today. We predict that the 470 Ma impact event is likely to be found on the Moon and Mars, if not Mercury.
C1 [Yin, Qing-Zhu] Univ Calif Davis, Dept Earth & Planetary Sci, Davis, CA 95616 USA.
[Zhou, Qin] Chinese Acad Sci, Natl Astron Observ, Key Lab Lunar & Deep Space Explorat, Beijing 100012, Peoples R China.
[Li, Qiu-Li; Li, Xian-Hua; Liu, Yu; Tang, Guo-Qiang] Chinese Acad Sci, Inst Geol & Geophys, State Key Lab Lithospher Evolut, Beijing 100029, Peoples R China.
[Krot, Alexander N.] Univ Hawaii Manoa, Hawaii Inst Geophys & Planetol, Honolulu, HI 96822 USA.
[Jenniskens, Peter] SETI Inst, Mountain View, CA 94043 USA.
[Jenniskens, Peter] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
RP Yin, QZ (reprint author), Univ Calif Davis, Dept Earth & Planetary Sci, One Shields Ave, Davis, CA 95616 USA.
EM qyin@ucdavis.edu
RI liu, yu/P-1081-2014; Yin, Qing-Zhu/B-8198-2009;
OI liu, yu/0000-0001-7195-7393; Yin, Qing-Zhu/0000-0002-4445-5096; Li,
Qiuli/0000-0002-7280-5508
FU NSFC grants [41222023, 41221002]
FX We sincerely thank Darci Kane for making the Novato N06 meteorite sample
available for this study. We thank the reviewers, P. Claeys, P. Heck,
and H. Hidaka, for their constructive comments and the associate editor
Gretchen Benedix and executive editor A. J. Timothy Jull and the
editorial office staff for their efficient handling of the manuscript.
QLL and XHL acknowledge support from NSFC grants 41222023 and 41221002.
NR 75
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U1 0
U2 7
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 1086-9379
EI 1945-5100
J9 METEORIT PLANET SCI
JI Meteorit. Planet. Sci.
PD AUG
PY 2014
VL 49
IS 8
BP 1426
EP 1439
DI 10.1111/maps.12340
PG 14
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA AN8SZ
UT WOS:000340875900008
ER
PT J
AU Udom, I
Zhang, YY
Ram, MK
Stefanakos, EK
Hepp, AF
Elzein, R
Schlaf, R
Goswami, DY
AF Udom, Innocent
Zhang, Yangyang
Ram, Manoj K.
Stefanakos, Elias K.
Hepp, Aloysius F.
Elzein, Radwan
Schlaf, Rudy
Goswami, D. Yogi
TI A simple photolytic reactor employing Ag-doped ZnO nanowires for water
purification
SO THIN SOLID FILMS
LA English
DT Article
DE Silver; Zinc oxide; Nanowires; Photoreactor; Water Purification
ID PHOTOCATALYTIC DEGRADATION; METHYL-ORANGE; NANORODS; PHOTODEGRADATION;
LIGHT; GROWTH; ARRAY; DISINFECTION; PERFORMANCE; SUSPENSIONS
AB Well-aligned native zinc oxide (ZnO) and silver-doped ZnO (Ag-ZnO) films were deposited on borosilicate glass via a simple, low-cost, low-temperature, scalable hydrothermal process. The as-synthesized ZnO and Ag-ZnO films were characterized by X-ray diffraction; scanning electron microscopy, UV-visible spectroscopy, and Fourier transform infrared spectroscopy. A simple photolytic reactor was fabricated and later used to find the optimum experimental conditions for photocatalytic performance. The photodegradation of methyl orange in water was investigated using as-prepared ZnO and Ag-ZnO nanowires, and was compared to P25 (a commercial photocatalyst) in both visible and UV radiations. The P25 and Ag-ZnO showed a similar photodegradation performance under UV light, but Ag-ZnO demonstrated superior photocatalytic activity under visible irradiation. The optimized doping of Ag in Ag-ZnO enhanced photocatalytic activity in a simple reactor design and indicated potential applicability of Ag-ZnO for large-scale purification of water under solar irradiation. (C) 2014 Elsevier B.V. All rights reserved.
C1 [Udom, Innocent; Zhang, Yangyang; Ram, Manoj K.; Stefanakos, Elias K.] Univ S Florida, Clean Energy Res Ctr, Coll Engn, Tampa, FL 33620 USA.
[Elzein, Radwan; Schlaf, Rudy] Univ S Florida, Dept Elect Engn, Tampa, FL 33620 USA.
[Hepp, Aloysius F.] Univ S Florida, Dept Chem & Biomed Engn, Tampa, FL 33620 USA.
[Goswami, D. Yogi] NASA Glenn Res Ctr, Res & Technol Directorate, Cleveland, OH 44135 USA.
RP Ram, MK (reprint author), Univ S Florida, Clean Energy Res Ctr, 4202 E Fowler Ave,ENB 118,Loc NTA102, Tampa, FL 33620 USA.
EM mkram@usf.edu
OI Ram, Manoj/0000-0002-6833-5566
FU National Aeronautics and Space Administration (NASA) - Harriett Jenkins
Pre-doctoral Fellowship; State of Florida through the Florida Energy
Systems Consortium (FESC) funds
FX This work was supported by the National Aeronautics and Space
Administration (NASA) - Harriett Jenkins Pre-doctoral Fellowship and the
State of Florida through the Florida Energy Systems Consortium (FESC)
funds.
NR 42
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U1 3
U2 41
PU ELSEVIER SCIENCE SA
PI LAUSANNE
PA PO BOX 564, 1001 LAUSANNE, SWITZERLAND
SN 0040-6090
J9 THIN SOLID FILMS
JI Thin Solid Films
PD AUG 1
PY 2014
VL 564
BP 258
EP 263
DI 10.1016/j.tsf.2014.05.057
PG 6
WC Materials Science, Multidisciplinary; Materials Science, Coatings &
Films; Physics, Applied; Physics, Condensed Matter
SC Materials Science; Physics
GA AN8KD
UT WOS:000340852200035
ER
PT J
AU Farnocchia, D
Chesley, SR
Tholen, DJ
Micheli, M
AF Farnocchia, D.
Chesley, S. R.
Tholen, D. J.
Micheli, M.
TI High precision predictions for near-Earth asteroids: the strange case of
(3908) Nyx
SO CELESTIAL MECHANICS & DYNAMICAL ASTRONOMY
LA English
DT Article
DE Astrometric treatment; Orbit determination; Asteroids; Yarkovsky effect;
Orbital drift
ID RADIATION PRESSURE; YARKOVSKY; CATALOG
AB In November 2004 radar delay measurements of near-Earth asteroid (3908) Nyx obtained at the Arecibo radio telescope turned out to be away from the orbital prediction. We prove that this discrepancy was caused by a poor astrometric treatment and an incomplete dynamical model, which did not account for nongravitational perturbations. To improve the astrometric treatment, we remove known star catalog biases, apply suitable weights to the observations, and use an aggressive outlier rejection scheme. The main issue related to the dynamical model is having not accounted for the Yarkovsky effect. Including the Yarkovsky perturbation in the model makes the orbital prediction and the radar measurements statistically consistent by both reducing the offset and increasing the prediction uncertainty to a more realistic level. This analysis shows the sensitivity of high precision predictions to the astrometric treatment and the Yarkovsky effect. By using the full observational dataset we obtain a detection of the Yarkovsky effect acting on Nyx corresponding to an orbital drift m/year. In turn, we derive constraints on thermal inertia and bulk density. In particular, we find that the bulk density of Nyx is around 1 g/cm, possibly less. To make sure that our results are not corrupted by an asteroid impact or a close approach with a perturbing asteroid not included in our dynamical model, we show that the astrometry provides no convincing evidence of an impulsive variation of Nyx's velocity while crossing the main belt region.
C1 [Farnocchia, D.; Chesley, S. R.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Tholen, D. J.; Micheli, M.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA.
RP Farnocchia, D (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM Davide.Farnocchia@jpl.nasa.gov
OI Micheli, Marco/0000-0001-7895-8209
FU NASA Postdoctoral Program at the Jet Propulsion Laboratory; California
Institute of Technology; NASA; U.S. National Science Foundation [AST
0709500, AST 1109940]
FX We thank Fabrizio Bernardi for obtaining and measuring some of the
observations in Table 5. DF was supported for this research by an
appointment to the NASA Postdoctoral Program at the Jet Propulsion
Laboratory, California Institute of Technology, administered by Oak
Ridge Associated Universities through a contract with NASA. SC conducted
this research at the Jet Propulsion Laboratory, California Institute of
Technology, under a contract with NASA. DT and MM were funded by Grants
AST 0709500 and AST 1109940 from the U.S. National Science 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 sacred mountain.
NR 28
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U1 0
U2 1
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0923-2958
EI 1572-9478
J9 CELEST MECH DYN ASTR
JI Celest. Mech. Dyn. Astron.
PD AUG
PY 2014
VL 119
IS 3-4
SI SI
BP 301
EP 312
DI 10.1007/s10569-014-9536-9
PG 12
WC Astronomy & Astrophysics; Mathematics, Interdisciplinary Applications
SC Astronomy & Astrophysics; Mathematics
GA AN3NQ
UT WOS:000340495600007
ER
PT J
AU da Costa, ET
Mora, MF
Willis, PA
do Lago, CL
Jiao, H
Garcia, CD
AF da Costa, Eric Tavares
Mora, Maria F.
Willis, Peter A.
do Lago, Claudimir L.
Jiao, Hong
Garcia, Carlos D.
TI Getting started with open-hardware: Development and control of
microfluidic devices
SO ELECTROPHORESIS
LA English
DT Article
DE Open-source; PDMS; Valves
ID MICROCHIP-CAPILLARY-ELECTROPHORESIS; CONTACTLESS CONDUCTIVITY DETECTION;
IN-SITU ANALYSIS; ELECTROCHEMICAL DETECTION; MASS-SPECTROMETRY; MEMBRANE
VALVES; FOOD ANALYSIS; PUMPS; INSTRUMENTATION; INTEGRATION
AB Understanding basic concepts of electronics and computer programming allows researchers to get the most out of the equipment found in their laboratories. Although a number of platforms have been specifically designed for the general public and are supported by a vast array of on-line tutorials, this subject is not normally included in university chemistry curricula. Aiming to provide the basic concepts of hardware and software, this article is focused on the design and use of a simple module to control a series of PDMS-based valves. The module is based on a low-cost microprocessor (Teensy) and open-source software (Arduino). The microvalves were fabricated using thin sheets of PDMS and patterned using CO2 laser engraving, providing a simple and efficient way to fabricate devices without the traditional photolithographic process or facilities. Synchronization of valve control enabled the development of two simple devices to perform injection (1.6 +/- 0.4 mu L/stroke) and mixing of different solutions. Furthermore, a practical demonstration of the utility of this system for microscale chemical sample handling and analysis was achieved performing an on-chip acid-base titration, followed by conductivity detection with an open-source low-cost detection system. Overall, the system provided a very reproducible (98%) platform to perform fluid delivery at the microfluidic scale.
C1 [da Costa, Eric Tavares; Garcia, Carlos D.] Univ Texas San Antonio, Dept Chem, San Antonio, TX 78248 USA.
[da Costa, Eric Tavares; do Lago, Claudimir L.] Univ Sao Paulo, Dept Quim Fundamental, Inst Quim, Sao Paulo, Brazil.
[Mora, Maria F.; Willis, Peter A.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Jiao, Hong] HJ Sci & Technol, Berkeley, CA USA.
RP Garcia, CD (reprint author), Univ Texas San Antonio, Dept Chem, One UTSA Circle, San Antonio, TX 78248 USA.
EM carlos.garcia@utsa.edu
RI do Lago, Claudimir/A-1852-2008; Mora, Maria/C-9753-2009; Institute of
Chemistry - USP, Dept. of Chemistry/B-8988-2012; Willis,
Peter/I-6621-2012; da Costa, Eric/D-5387-2012; Garcia,
Carlos/A-8681-2008
OI do Lago, Claudimir/0000-0003-1542-4343; da Costa,
Eric/0000-0003-4489-3501; Garcia, Carlos/0000-0002-7583-5585
FU NASA STTR [NNX13CP49C]; University of Texas at San Antonio; National
Institutes of Health through the Research Centers at Minority
Institutions [G12MD007591]
FX The authors gratefully acknowledge the financial support provided by
NASA STTR (Contract number: NNX13CP49C), The University of Texas at San
Antonio, and the National Institutes of Health through the Research
Centers at Minority Institutions (G12MD007591).
NR 50
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U1 8
U2 66
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 0173-0835
EI 1522-2683
J9 ELECTROPHORESIS
JI Electrophoresis
PD AUG
PY 2014
VL 35
IS 16
SI SI
BP 2370
EP 2377
DI 10.1002/elps.201400128
PG 8
WC Biochemical Research Methods; Chemistry, Analytical
SC Biochemistry & Molecular Biology; Chemistry
GA AN2DU
UT WOS:000340394800013
PM 24823494
ER
PT J
AU Bakermans, C
Skidmore, ML
Douglas, S
McKay, CP
AF Bakermans, Corien
Skidmore, Mark L.
Douglas, Susanne
McKay, Christopher P.
TI Molecular characterization of bacteria from permafrost of the Taylor
Valley, Antarctica
SO FEMS MICROBIOLOGY ECOLOGY
LA English
DT Article
DE 16S rRNA gene; rpoB; cold adaptation; psychrophiles
ID MCMURDO DRY VALLEYS; 16S RIBOSOMAL-RNA; AT-15 DEGREES-C; SIBERIAN
PERMAFROST; MICROBIAL DIVERSITY; COLD ADAPTATION; GROWTH TEMPERATURES;
VICTORIA LAND; PSYCHROPHILIC ENZYMES; COMMUNITY STRUCTURE
AB While bacterial communities from McMurdo Dry Valley soils have been studied using molecular techniques, data from permafrost are particularly scarce given the logistical difficulties of sampling. This study examined the molecular diversity and culturability of bacteria in permafrost from the Taylor Valley (TV), Antarctica. A 16S rRNA gene clone library was constructed to assess bacterial diversity, while a clone library of the RNA polymerase beta subunit (rpoB) gene was constructed to examine amino acid composition of an essential protein-coding gene. The 16S rRNA gene clone library was dominated by Acidobacteria from Gp6 and Gemmatimonadetes. The rpoB gene clone library (created with primers designed in this study) was also dominated by Acidobacteria. The ability of sequence analyses to garner additional information about organisms represented by TV sequences was explored. Specifically, optimum growth temperature was estimated from the stem GC content of the 16S rRNA gene, while potential cold adaptations within translated rpoB sequences were assessed. These analyses were benchmarked using known psychrophiles and mesophiles. Bioinformatic analyses suggested that many TV sequences could represent organisms capable of activity at low temperatures. Plate counts confirmed that c. 10(3) cells per gram permafrost remained viable and were culturable, while laboratory respiration assays demonstrated that microbial activity occurred at -5 degrees C and peaked at 15 degrees C.
C1 [Bakermans, Corien] Penn State Univ, Altoona Coll, Altoona, PA 16601 USA.
[Skidmore, Mark L.] Montana State Univ, Bozeman, MT 59717 USA.
[Douglas, Susanne] Planetary Sci Inst, Tucson, AZ USA.
[McKay, Christopher P.] NASA Ames Res Ctr, Moffett Field, CA USA.
RP Bakermans, C (reprint author), Penn State Univ, Altoona Coll, 3000 Ivyside Pk, Altoona, PA 16601 USA.
EM cub21@psu.edu
FU Penn State; NASA; NSF [0525567, 0636770]; NASA Astrobiology Science and
Technology for Exploring Planets (ASTEP) program
FX This study was supported by internal grants from Penn State to C.B. C.B.
was also partially supported by a NASA Montana Space Grant and NSF
0525567. M. S. was partially supported by NSF Grants 0525567 and
0636770. Sample collection was supported by a NASA International Polar
Year grant to Dr Leslie Tamppari, which supported C.P.M. S.D. was
supported by the NASA Astrobiology Science and Technology for Exploring
Planets (ASTEP) program. Many thanks to Penn State Altoona undergraduate
students S. Gorman, S. Abbott, F. Wendt, and E. Malmberg.
NR 109
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U1 1
U2 41
PU OXFORD UNIV PRESS
PI OXFORD
PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND
SN 0168-6496
EI 1574-6941
J9 FEMS MICROBIOL ECOL
JI FEMS Microbiol. Ecol.
PD AUG
PY 2014
VL 89
IS 2
SI SI
BP 331
EP 346
DI 10.1111/1574-6941.12310
PG 16
WC Microbiology
SC Microbiology
GA AN4CM
UT WOS:000340535200011
PM 24592998
ER
PT J
AU Guilbert, J
Beckage, B
Winter, JM
Horton, RM
Perkins, T
Bomblies, A
AF Guilbert, Justin
Beckage, Brian
Winter, Jonathan M.
Horton, Radley M.
Perkins, Timothy
Bomblies, Arne
TI Impacts of Projected Climate Change over the Lake Champlain Basin in
Vermont
SO JOURNAL OF APPLIED METEOROLOGY AND CLIMATOLOGY
LA English
DT Article
ID FOREST ECOSYSTEMS; MODEL PROJECTIONS; PRECIPITATION; TEMPERATURE;
HUMIDITY; DATABASE; UTILITY; TRENDS; ICE
AB The Lake Champlain basin is a critical ecological and socioeconomic resource of the northeastern United States and southern Quebec, Canada. While general circulation models (GCMs) provide an overview of climate change in the region, they lack the spatial and temporal resolution necessary to fully anticipate the effects of rising global temperatures associated with increasing greenhouse gas concentrations. Observed trends in precipitation and temperature were assessed across the Lake Champlain basin to bridge the gap between global climate change and local impacts. Future shifts in precipitation and temperature were evaluated as well as derived indices, including maple syrup production, days above 32.2 degrees C (90 degrees F), and snowfall, relevant to managing the natural and human environments in the region. Four statistically downscaled, bias-corrected GCM simulations were evaluated from the Coupled Model Intercomparison Project phase 5 (CMIP5) forced by two representative concentration pathways (RCPs) to sample the uncertainty in future climate simulations. Precipitation is projected to increase by between 9.1 and 12.8 mm yr(-1) decade(-1) during the twenty-first century while daily temperatures are projected to increase between 0.43 degrees and 0.49 degrees C decade(-1). Annual snowfall at six major ski resorts in the region is projected to decrease between 46.9% and 52.4% by the late twenty-first century. In the month of July, the number of days above 32.2 degrees C in Burlington, Vermont, is projected to increase by over 10 days during the twenty-first century.
C1 [Guilbert, Justin; Bomblies, Arne] Univ Vermont, Sch Engn, Burlington, VT USA.
[Beckage, Brian; Perkins, Timothy] Univ Vermont, Dept Plant Biol, Burlington, VT USA.
[Winter, Jonathan M.; Horton, Radley M.] Columbia Univ, Earth Inst, Ctr Climate Syst Res, New York, NY USA.
[Horton, Radley M.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
RP Guilbert, J (reprint author), 23 Mansfield Ave, Burlington, VT 05401 USA.
EM jguilber@uvm.edu
FU Vermont EPSCoR through NSF [EPS-1101317]
FX This work was supported by Vermont EPSCoR through NSF Award EPS-1101317.
Many thanks are given to Levi Brekke, Ed Maurer, and Tom Pruitt for
their assistance with the BCCA data used in this analysis.
NR 34
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U1 1
U2 33
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 AUG
PY 2014
VL 53
IS 8
BP 1861
EP 1875
DI 10.1175/JAMC-D-13-0338.1
PG 15
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA AN3TS
UT WOS:000340512200001
ER
PT J
AU Swimmer, Y
Campora, CE
Mcnaughton, L
Musyl, M
Parga, M
AF Swimmer, Y.
Campora, C. Empey
Mcnaughton, L.
Musyl, M.
Parga, M.
TI Post-release mortality estimates of loggerhead sea turtles (Caretta
caretta) caught in pelagic longline fisheries based on satellite data
and hooking location
SO AQUATIC CONSERVATION-MARINE AND FRESHWATER ECOSYSTEMS
LA English
DT Article
DE bycatch; telemetry; post-release mortality; sea turtles
ID CIRCLE HOOKS; TRACKING TURTLES; BYCATCH; MARINE; CATCH; SURVIVAL;
CAPTURE; REDUCE; DEATH; OCEAN
AB 1. There are few reliable estimates of post-release mortality for sea turtle species because of the many challenges and costs associated with tracking animals released at sea. In this study, the likelihood of sea turtle mortality as a result of interactions with longline fishing gear was estimated based on satellite telemetry data, such as the number of days an animal was successfully tracked, or days at liberty (DAL) and dive depth data, as well as anatomical hooking locations.
2. Pop-up satellite archival tags were deployed on 29 loggerhead sea turtles (Caretta caretta) caught by the North Pacific US-based pelagic longline fishery operating from California and Hawaii between 2002 and 2006. Loggerhead turtles were catagorized by observers as shallow-hooked (55%) if the animal was entangled in the line or the hook was in the flipper, jaw or mouth and could be removed, or deep-hooked (45%) if the hook was ingested and could not be removed. The vertical movements of turtles were used to infer potential mortalities.
3. Of the 25 tags that reported data, the DAL ranged from 3 to 243 days (mean = 68 days). The DAL was shorter (by nearly 50%) for shallow-hooked (mean = 48 days, range: 3 to 127) compared to deep-hooked turtles (mean = 94 days, range: 5 to 243), but these changes were not statistically significant (P = 0.0658).
4. Although aspects of these analyses may be considered speculative, these data provide empirical evidence to indicate that deep-hooking is not linked to shorter DAL.
5. DAL, anatomical hooking location, and gear removal were evaluated with inferences about the extent of injuries and rates of infection to estimate an overall post-release mortality rate of 28% (95% bootstrap CI: 16-52%).
6. This range of estimates is consistent with those used to shape some US fisheries management plans, suggesting that conservation goals are being achieved at the expected level and ideally striking a balance between the interests of industry and those of protected species. Copyright (C) 2013 John Wiley & Sons, Ltd.
C1 [Swimmer, Y.] Natl Marine Fisheries Serv, Pacific Isl Fisheries Sci Ctr, Honolulu, HI 96822 USA.
[Campora, C. Empey] Biolintec Consulting LLC, Kailua, HI USA.
[Mcnaughton, L.; Musyl, M.] Univ Hawaii, Joint Inst Marine & Atmospher Res, Honolulu, HI 96822 USA.
[Musyl, M.] Pelag Res Grp LLC, Honolulu, HI USA.
[Parga, M.] SUBMON, Barcelona, Spain.
RP Swimmer, Y (reprint author), Natl Marine Fisheries Serv, Pacific Isl Fisheries Sci Ctr, Honolulu, HI 96822 USA.
EM yonat.swimmer@noaa.gov
FU University of Hawaii Pelagic Fisheries Research Program [658847];
Pacific Islands Fisheries Science Center (NOAA, US National Marine
Fisheries Service)
FX We thank the fisheries observers, coordinators, vessel owners and crew
involved in this project. We are also grateful to C. Boggs, L. Nakamura,
D. Lau and J. Sibert for extensive technical and administrative
assistance. This project was funded by the University of Hawaii Pelagic
Fisheries Research Program (Grant #658847) and the Pacific Islands
Fisheries Science Center (NOAA, US National Marine Fisheries Service).
All research was conducted in accordance with the protocols and handling
guidelines set forth by the University of Hawaii Animal Care and Use
Committee (IACUC Protocol #00-037-2). The views expressed herein are
those of the authors and do not necessarily reflect the views of NOAA of
any of its subdivisions.
NR 45
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U1 4
U2 39
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 1052-7613
EI 1099-0755
J9 AQUAT CONSERV
JI Aquat. Conserv.-Mar. Freshw. Ecosyst.
PD AUG
PY 2014
VL 24
IS 4
BP 498
EP 510
DI 10.1002/aqc.2396
PG 13
WC Environmental Sciences; Marine & Freshwater Biology; Water Resources
SC Environmental Sciences & Ecology; Marine & Freshwater Biology; Water
Resources
GA AN0BR
UT WOS:000340247200005
ER
PT J
AU Olsen, JL
Coyer, JA
Chesney, B
AF Olsen, Jeanine L.
Coyer, James A.
Chesney, Bryant
TI Numerous mitigation transplants of the eelgrass Zostera marina in
southern California shuffle genetic diversity and may promote
hybridization with Zostera pacifica
SO BIOLOGICAL CONSERVATION
LA English
DT Article
DE Admixture; Diversity; Genetics; Hybridization; Management; Transplants
ID COASTAL BAY SYSTEM; GENOTYPIC DIVERSITY; POPULATION-STRUCTURE;
MICROSATELLITE LOCI; CLONAL ORGANISMS; F-STATISTICS; RECOVERY; DISTANCE;
DISTURBANCE; DOMINANCE
AB Intensive human pressures along the southern California coast have led to >50 mitigation transplants of eelgrass over the past 30 years. We analyzed diversity and population structure of Zostera marina and Zostera pacifica at 36 locations to identify potential management units and further develop transplant guidelines. Normalized allelic diversity of Z. marina was uniformly moderate to high (4.78; 3.48-6.44) and nearly twofold higher than mainland Z. pacifica (2.70; 1.74-4.89). More than half of the Z. marina populations exhibited strongly significant inbreeding coefficients coupled with strong linkage disequilibrium attributable to transplant effects; neither attribute was found in Z. pacifica. Both species were characterized by high genotypic diversity and an absence of large clones. A Bayesian analysis of population structure suggested 6 potential management units for Z. marina and 3 for Z. pacifica; some units included disjunct locations associated with transplants. Hybridization between Z. marina and Z. pacifica Was documented at Newport Bay Entrance Channel and south San Diego Bay. The presence of two species requires management plans for each, as well as avoidance of potential transplant-induced hybridization. Although transplant admixtures elevate diversity, shuffling among locations may potentially reduce the genetic potential necessary to ensure rapid adaptation, even though overall transplant success has been successful. Given that transplants will continue (from both plants and seeds), we recommend that the current requirement for "two additional distinct donor sites" be restricted to within a management unit for small, routine mitigations and expanded to among-management units for wholesale de novo restorations. (C) 2014 Elsevier Ltd. All rights reserved.
C1 [Olsen, Jeanine L.] Univ Groningen, Ctr Ecol & Evolutionary Studies, Marine Benth Ecol & Evolut Grp, NL-9700 CC Groningen, Netherlands.
[Coyer, James A.] Cornell Univ, Shoals Marine Lab, Portsmouth, NH 03801 USA.
[Chesney, Bryant] Natl Marine Fisheries Serv, NOAA, Habitat Conservat Div, Long Beach, CA 90802 USA.
RP Olsen, JL (reprint author), Univ Groningen, Ctr Ecol & Evolutionary Studies, Marine Benth Ecol & Evolut Grp, Postbus 11103,Nijenborgh 7, NL-9700 CC Groningen, Netherlands.
EM j.l.olsen@rug.nl
FU NOAA - USA via Western Regional Acquisition Division, Southwest Region,
NMFS, Long Beach, CA [NFFR5400-11-04308]
FX We thank Adam Obaza, Eric Chavez and the Santa Barbara Channelkeeper for
the California collections: and Lydia Ladah for the Mexican collections.
We also thank Jan Veldsink for technical assistance in the laboratory
and Per Palsboll for discussions about linkage disequilibrium. This work
was supported by NOAA - USA Grant (NFFR5400-11-04308) to JLO via the
Western Regional Acquisition Division, Southwest Region, NMFS, Long
Beach, CA. The views expressed herein do not necessarily reflect the
view of those organizations.
NR 80
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U1 3
U2 36
PU ELSEVIER SCI LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND
SN 0006-3207
EI 1873-2917
J9 BIOL CONSERV
JI Biol. Conserv.
PD AUG
PY 2014
VL 176
BP 133
EP 143
DI 10.1016/j.biocon.2014.05.001
PG 11
WC Biodiversity Conservation; Ecology; Environmental Sciences
SC Biodiversity & Conservation; Environmental Sciences & Ecology
GA AM9TI
UT WOS:000340223500015
ER
PT J
AU Fletcher, JM
Teran, OJ
Rockwell, TK
Oskin, ME
Hudnut, KW
Mueller, KJ
Spelz, RM
Akciz, SO
Masana, E
Faneros, G
Fielding, EJ
Leprince, S
Morelan, AE
Stock, J
Lynch, DK
Elliott, AJ
Gold, P
Liu-Zeng, J
Gonzalez-Ortega, A
Hinojosa-Corona, A
Gonzalez-Garcia, J
AF Fletcher, John M.
Teran, Orlando J.
Rockwell, Thomas K.
Oskin, Michael E.
Hudnut, Kenneth W.
Mueller, Karl J.
Spelz, Ronald M.
Akciz, Sinan O.
Masana, Eulalia
Faneros, Geoff
Fielding, Eric J.
Leprince, Sebastien
Morelan, Alexander E.
Stock, Joann
Lynch, David K.
Elliott, Austin J.
Gold, Peter
Liu-Zeng, Jing
Gonzalez-Ortega, Alejandro
Hinojosa-Corona, Alejandro
Gonzalez-Garcia, Javier
TI Assembly of a large earthquake from a complex fault system: Surface
rupture kinematics of the 4 April 2010 El Mayor-Cucapah (Mexico) M-w 7.2
earthquake
SO GEOSPHERE
LA English
DT Article
ID SAN-ANDREAS FAULT; GULF-OF-CALIFORNIA; AMERICA PLATE BOUNDARY;
LAGUNA-SALADA FAULT; ANGLE NORMAL-FAULT; SOUTHERN-CALIFORNIA;
BAJA-CALIFORNIA; SHEAR ZONE; EASTERN CALIFORNIA; DIPPING FAULTS
AB The 4 April 2010 moment magnitude (M-w) 7.2 El Mayor-Cucapah earthquake revealed the existence of a previously unidentified fault system in Mexico that extends similar to 120 km from the northern tip of the Gulf of California to the U.S.-Mexico border. The system strikes northwest and is composed of at least seven major faults linked by numerous smaller faults, making this one of the most complex surface ruptures ever documented along the Pacific-North America plate boundary. Rupture propagated bilaterally through three distinct kinematic and geomorphic domains. Southeast of the epicenter, a broad region of distributed fracturing, liquefaction, and discontinuous fault rupture was controlled by a buried, southwest-dipping, dextral-normal fault system that extends similar to 53 km across the southern Colorado River delta. Northwest of the epicenter, the sense of vertical slip reverses as rupture propagated through multiple strands of an imbricate stack of east-dipping dextral-normal faults that extend similar to 55 km through the Sierra Cucapah. However, some coseismic slip (10-30 cm) was partitioned onto the west-dipping Laguna Salada fault, which extends parallel to the main rupture and defines the western margin of the Sierra Cucapah. In the northernmost domain, rupture terminates on a series of several north-northeast-striking cross-faults with minor offset (<8 cm) that cut uplifted and folded sediments of the northern Colorado River delta in the Yuha Desert.
In the Sierra Cucapah, primary rupture occurred on four major faults separated by one fault branch and two accommodation zones. The accommodation zones are distributed in a left-stepping en echelon geometry, such that rupture passed systematically to structurally lower faults. The structurally lowest fault that ruptured in this event is inclined as shallowly as similar to 20. Net surface offsets in the Sierra Cucapah average similar to 200 cm, with some reaching 300-400 cm, and rupture kinematics vary greatly along strike. Nonetheless, instantaneous extension directions are consistently oriented similar to 085 and the dominant slip direction is similar to 310, which is slightly (similar to 10) more westerly than the expected azimuth of relative plate motion, but considerably more oblique to other nearby historical ruptures such as the 1992 Landers earthquake. Complex multifault ruptures are common in the central portion of the Pacific North American plate margin, which is affected by restraining bend tectonics, gravitational potential energy gradients, and the inherently three-dimensional strain of the transtensional and transpressional shear regimes that operate in this region.
C1 [Fletcher, John M.; Teran, Orlando J.; Gonzalez-Ortega, Alejandro; Hinojosa-Corona, Alejandro; Gonzalez-Garcia, Javier] Ctr Inves Cient & Educ Super Ensenada, Dept Geol, Ensenada 22860, Baja California, Mexico.
[Rockwell, Thomas K.; Faneros, Geoff] San Diego State Univ, Dept Geol Sci, San Diego, CA 92182 USA.
[Oskin, Michael E.; Morelan, Alexander E.; Elliott, Austin J.; Gold, Peter] Univ Calif Davis, Dept Earth & Planetary Sci, Davis, CA 95616 USA.
[Hudnut, Kenneth W.; Lynch, David K.] US Geol Survey, Pasadena, CA 91106 USA.
[Mueller, Karl J.] Univ Colorado, Dept Geol Sci, Boulder, CO 80309 USA.
[Spelz, Ronald M.] Univ Autonoma Baja California, Fac Ciencias Marinas, Ensenada 22860, Baja California, Mexico.
[Akciz, Sinan O.] Univ Calif Los Angeles, Dept Earth Planetary & Space Sci, Los Angeles, CA 90095 USA.
[Masana, Eulalia] Univ Barcelona, Dept Geodinam & Geofis, E-08028 Barcelona, Spain.
[Fielding, Eric J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Leprince, Sebastien; Stock, Joann] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA.
[Liu-Zeng, Jing] China Earthquake Adm, Inst Geol, State Key Lab Earthquake Dynam, Beijing 100029, Peoples R China.
RP Fletcher, JM (reprint author), Ctr Inves Cient & Educ Super Ensenada, Dept Geol, Carretera Tijuana Ensenada,3918 Zona Playitas, Ensenada 22860, Baja California, Mexico.
EM jfletche@cicese.mx
RI Masana, Eulalia/I-2122-2015; Hudnut, Kenneth/B-1945-2009; Liu-Zeng,
Jing/F-8582-2011; Hinojosa-Corona, Alejandro/L-5422-2015;
OI Masana, Eulalia/0000-0001-8315-7561; Hudnut,
Kenneth/0000-0002-3168-4797; Hinojosa-Corona,
Alejandro/0000-0002-2282-337X; Rockwell, Thomas/0000-0001-5319-6447;
Stock, Joann Miriam/0000-0003-4816-7865
FU CONACYT (Consejo Nacional de Ciencia y Tecnologia) [81463]; SCEC
(Southern California Earthquake Center) [1697]; National Science
Foundation [EAR-0529922]; GEER (Geotechnical Extreme Events
Reconnaissance) Foundation; Keck Institute for Space Studies; Gordon and
Betty Moore Foundation; National Aeronautics and Space Administration
(NASA) Earth Surface and Interior focus area; NASA
FX This work was financed by CONACYT (Consejo Nacional de Ciencia y
Tecnologia) grant 81463, SCEC (Southern California Earthquake Center)
grant 1697, and National Science Foundation grant EAR-0529922; the GEER
(Geotechnical Extreme Events Reconnaissance) Foundation provided funding
for initial field work. S. Leprince was supported in part by the Keck
Institute for Space Studies and by the Gordon and Betty Moore
Foundation. Part of this study was sponsored by the National Aeronautics
and Space Administration (NASA) Earth Surface and Interior focus area
and performed at the Jet Propulsion Laboratory, California Institute of
Technology, under contract with NASA. Enlightening discussions with Paul
Wetmore and Francisco Suarez helped refine ideas about tectonics of the
Big Bend domain and the kinematics of faulting in the Colorado River
delta, respectively. We thank John Galetzka, Kate Scharer, David Bowman,
Roman Manjarrez, and Maria Oturno for help with field work. We also
thank Jose Mojarro, Sergio Arregui, and Luis Gradilla for technical
support.
NR 82
TC 21
Z9 21
U1 2
U2 27
PU GEOLOGICAL SOC AMER, INC
PI BOULDER
PA PO BOX 9140, BOULDER, CO 80301-9140 USA
SN 1553-040X
J9 GEOSPHERE
JI Geosphere
PD AUG
PY 2014
VL 10
IS 4
BP 797
EP 827
DI 10.1130/GES00933.1
PG 31
WC Geosciences, Multidisciplinary
SC Geology
GA AM6GK
UT WOS:000339961500010
ER
PT J
AU Murri, GB
AF Murri, Gretchen B.
TI Effect of data reduction and fiber-bridging on Mode I delamination
characterization of unidirectional composites
SO JOURNAL OF COMPOSITE MATERIALS
LA English
DT Article
DE Composites; fracture toughness; fatigue; Paris Law; delamination; strain
energy release rate; R-curve
AB Reliable delamination characterization data for laminated composites are needed for input in analytical models of structures to predict delamination onset and growth. The double-cantilevered beam specimen is used to measure fracture toughness, G(Ic), and strain energy release rate, G(Imax), for delamination onset and growth in laminated composites under Mode I loading. The current study was conducted as part of an ASTM Round Robin activity to evaluate a proposed testing standard for Mode I fatigue delamination propagation. Static and fatigue tests were conducted on specimens of IM7/977-3 and G40-800/5276-1 graphite/epoxies, and S2/5216 glass/epoxy double-cantilevered beam specimens to evaluate the draft standard "Standard Test Method for Mode I Fatigue Delamination Propagation of Unidirectional Fiber-Reinforced Polymer Matrix Composites." Static results were used to generate a delamination resistance curve, G(IR), for each material, which was used to determine the effects of fiber-bridging on the delamination growth data. All three materials were tested in fatigue at a cyclic G(Imax) level equal to 90% of the fracture toughness, G(Ic), to determine the delamination growth rate. Two different data reduction methods, a two-point and a seven-point fit, were used and the resulting Paris Law equations were compared. Growth rate results were normalized by the delamination resistance curve for each material and compared to the non-normalized results. Paris Law exponents were found to decrease by 5.7 to 47.6% due to normalizing the growth data. Additional specimens of the IM7/977-3 material were tested at three lower cyclic G(Imax) levels to compare the effect of loading level on delamination growth rates. The IM7/977-3 tests were also used to determine the delamination threshold curve for that material. The results show that tests at a range of loading levels are necessary to describe the complete delamination behavior of this material.
C1 NASA Langley Res Ctr, Hampton, VA 23681 USA.
RP Murri, GB (reprint author), NASA Langley Res Ctr, 2W Reid St,MS188E, Hampton, VA 23681 USA.
EM gretchen.b.murri@nasa.gov
NR 11
TC 7
Z9 7
U1 3
U2 12
PU SAGE PUBLICATIONS LTD
PI LONDON
PA 1 OLIVERS YARD, 55 CITY ROAD, LONDON EC1Y 1SP, ENGLAND
SN 0021-9983
EI 1530-793X
J9 J COMPOS MATER
JI J. Compos Mater.
PD AUG
PY 2014
VL 48
IS 19
BP 2413
EP 2424
DI 10.1177/0021998313498791
PG 12
WC Materials Science, Composites
SC Materials Science
GA AM9MZ
UT WOS:000340207000010
ER
PT J
AU Porcar-Castell, A
Tyystjarvi, E
Atherton, J
van der Tol, C
Flexas, J
Pfundel, EE
Moreno, J
Frankenberg, C
Berry, JA
AF Porcar-Castell, Albert
Tyystjarvi, Esa
Atherton, Jon
van der Tol, Christiaan
Flexas, Jaume
Pfuendel, Erhard E.
Moreno, Jose
Frankenberg, Christian
Berry, Joseph A.
TI Linking chlorophyll a fluorescence to photosynthesis for remote sensing
applications: mechanisms and challenges
SO JOURNAL OF EXPERIMENTAL BOTANY
LA English
DT Review
DE Gross primary production; GPP; leaf level; photosystem II; photosystem
I; PSII; PSI; photosynthesis dynamics; pulse amplitude modulation; PAM;
PSII connectivity; remote sensing; solar-induced fluorescence;
sun-induced fluorescence; SIF
ID THERMAL-ENERGY DISSIPATION; LIGHT-USE EFFICIENCY; PHOTOCHEMICAL
REFLECTANCE INDEX; PIGMENT-PROTEIN COMPLEXES; PINUS-SYLVESTRIS L.;
THYLAKOID MEMBRANE ORGANIZATION; PHOTOSYSTEM-II FLUORESCENCE; ADJUSTED
VEGETATION INDEX; GROSS PRIMARY PRODUCTION; CARBON-DIOXIDE UPTAKE
AB Chlorophyll a fluorescence (ChlF) has been used for decades to study the organization, functioning, and physiology of photosynthesis at the leaf and subcellular levels. ChlF is now measurable from remote sensing platforms. This provides a new optical means to track photosynthesis and gross primary productivity of terrestrial ecosystems. Importantly, the spatiotemporal and methodological context of the new applications is dramatically different compared with most of the available ChlF literature, which raises a number of important considerations. Although we have a good mechanistic understanding of the processes that control the ChlF signal over the short term, the seasonal link between ChlF and photosynthesis remains obscure. Additionally, while the current understanding of in vivo ChlF is based on pulse amplitude-modulated (PAM) measurements, remote sensing applications are based on the measurement of the passive solar-induced chlorophyll fluorescence (SIF), which entails important differences and new challenges that remain to be solved. In this review we introduce and revisit the physical, physiological, and methodological factors that control the leaf-level ChlF signal in the context of the new remote sensing applications. Specifically, we present the basis of photosynthetic acclimation and its optical signals, we introduce the physical and physiological basis of ChlF from the molecular to the leaf level and beyond, and we introduce and compare PAM and SIF methodology. Finally, we evaluate and identify the challenges that still remain to be answered in order to consolidate our mechanistic understanding of the remotely sensed SIF signal.
C1 [Porcar-Castell, Albert; Atherton, Jon] Univ Helsinki, Dept Forest Sci, FIN-00014 Helsinki, Finland.
[Tyystjarvi, Esa] Univ Turku, Dept Biochem, FI-20014 Turku, Finland.
[van der Tol, Christiaan] Univ Twente, Fac ITC, NL-7524 AE Enschede, Netherlands.
[Flexas, Jaume] Univ Illes Balears, Palma De Mallorca 07122, Spain.
[Pfuendel, Erhard E.] Heinz Walz GmbH, D-91090 Effeltrich, Germany.
[Moreno, Jose] Univ Valencia, Fac Phys, Dept Earth Phys & Thermodynam, E-46100 Valencia, Spain.
[Frankenberg, Christian] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Berry, Joseph A.] Carnegie Inst Sci, Dept Global Ecol, Stanford, CA 94305 USA.
RP Porcar-Castell, A (reprint author), Univ Helsinki, Dept Forest Sci, POB 27, FIN-00014 Helsinki, Finland.
EM joan.porcar@helsinki.fi
RI Flexas, Jaume/C-1898-2012; Tyystjarvi, Esa/B-2360-2015; van der Tol,
Christiaan/A-2403-2010; Frankenberg, Christian/A-2944-2013;
OI Tyystjarvi, Esa/0000-0001-6808-7470; van der Tol,
Christiaan/0000-0002-2484-8191; Frankenberg,
Christian/0000-0002-0546-5857; Porcar-Castell,
Albert/0000-0003-1357-9982
FU Academy of Finland [1138884, 272041, 259075]; University of Helsinki
[490116]
FX This work has been supported by the Academy of Finland [grant nos
1138884 and 272041 to AP-C and 259075 to ET], and the University of
Helsinki (grant no 490116). This review idea originated from discussions
during a Workshop organized by the Keck Institute for Space Studies 'New
Methods for Measurements of Photosynthesis from Space'. The availability
of results from ongoing preparatory studies for the ESA FLEX mission is
acknowledged. We thank Professor Kari Heliovaara for help in preparing
Figs 2, 4, and 7.
NR 270
TC 64
Z9 65
U1 30
U2 207
PU OXFORD UNIV PRESS
PI OXFORD
PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND
SN 0022-0957
EI 1460-2431
J9 J EXP BOT
JI J. Exp. Bot.
PD AUG
PY 2014
VL 65
IS 15
BP 4065
EP 4095
DI 10.1093/jxb/eru191
PG 31
WC Plant Sciences
SC Plant Sciences
GA AM6EB
UT WOS:000339954300001
PM 24868038
ER
PT J
AU di Lauro, C
Lattanzi, F
Brown, LR
Soon, K
Mantz, AW
Smith, MAH
AF di Lauro, Carlo
Lattanzi, Franca
Brown, Linda R.
Soon, Keeyoon
Mantz, Arlan W.
Smith, Mary Ann H.
TI The V-4, V-9, V-10 and V-6+V-11 bands of (CH3CH3)-C-12-C-13 between 1345
and 1557 cm(-1)
SO JOURNAL OF MOLECULAR SPECTROSCOPY
LA English
DT Article
DE Line positions; Intensities; (CH3CH3)-C-12-C-13; Cold temperature;
Coriolis coupling; Torsional splitting; K-doubling
ID STIMULATED RAMAN-SPECTRUM; INTERNAL-ROTATION; LINE PARAMETERS; MU-M;
ETHANE; C2H6; (C2H6)-C-12; MOLECULE; REGION; TITAN
AB The infrared spectrum of (CH3CH3)-C-12-C-13 is measured between 1345 and 1560 cm(-1) using high resolution FTIR with a C-13-enriched gas sample cooled to 130.3 K. The three fundamentals v(4), v(9) and v(10) (at 1374, 1470 and 1468 cm-1 respectively) and one combination band v(6) + v(11) at 1473 cm-1 are analyzed for the first time. The transitions of v10 (an infrared inactive "g" mode of the ethane) are observed through its resonant coupling with v9 (corresponding to a "u" mode of normal ethane). Transitions of v(6) + v(11) are seen due to its strong coupling to v9. In general, torsional splitting produces two components (as in normal ethane), but in both v9 and v50, there is an additional small splitting of these components with degenerate torsional symmetry wherever the interacting v(10) levels become infrared active (from "g 4-* u" mixing); this mechanism is investigated. Several e-type resonances with AE = 2 and Ak = +1 are observed within v9 and between v(9) and v(10) while the strong interaction between v(9) and v(6) + v(11) plays a role in tuning pairs of levels into resonance. As in normal ethane, a detectable K-doubling occurs in the levels k= 2, e = 1 of v(9), and the parallel band v4 shows an intensity bias, with the R-transitions markedly stronger than the P-transitions, due to its x,y-Coriolis coupling with v9. The spectrum is analyzed by adopting an appropriate Hamiltonian model, and vibration-rotation-torsion parameters of the four mentioned vibrational states are determined by the least squares process using 1350 observed transition line positions (RMS deviation 3.24 x 10-3 cm-I). The values of rotational and torsional parameters of the vibrational ground state are also improved or determined anew, from data of the present spectrum. Two supplemental files are provided. One shows the fit of line positions, and the other gives the measured positions and intensities at 130 K (with known quantum assignments and lower state energies) so that lines of this molecule can be identified in planetary spectra. (C) 2014 Elsevier Inc. All rights reserved.
C1 [di Lauro, Carlo; Lattanzi, Franca] Univ Naples Federico II, I-80131 Naples, Italy.
[Brown, Linda R.; Soon, Keeyoon] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Mantz, Arlan W.] Connecticut Coll, Dept Phys Astron & Geophys, New London, CT 06320 USA.
[Smith, Mary Ann H.] NASA Langley Res Ctr, Sci Directorate, Hampton, VA 23681 USA.
RP Brown, LR (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM linda.r.brown@jpl.nasa.gov
RI Sung, Keeyoon/I-6533-2015
NR 34
TC 2
Z9 2
U1 1
U2 9
PU ACADEMIC PRESS INC ELSEVIER SCIENCE
PI SAN DIEGO
PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA
SN 0022-2852
EI 1096-083X
J9 J MOL SPECTROSC
JI J. Mol. Spectrosc.
PD AUG
PY 2014
VL 302
BP 36
EP 49
DI 10.1016/j.jms.2014.06.001
PG 14
WC Physics, Atomic, Molecular & Chemical; Spectroscopy
SC Physics; Spectroscopy
GA AM7CF
UT WOS:000340021600006
ER
PT J
AU Kim, JH
Chun, HY
Sharman, RD
Trier, SB
AF Kim, Jung-Hoon
Chun, Hye-Yeong
Sharman, Robert D.
Trier, Stanley B.
TI The Role of Vertical Shear on Aviation Turbulence within Cirrus Bands of
a Simulated Western Pacific Cyclone
SO MONTHLY WEATHER REVIEW
LA English
DT Article
ID CLEAR-AIR TURBULENCE; MESOSCALE CONVECTIVE SYSTEM; UPPER-LEVEL OUTFLOW;
CLOUD BANDS; MODEL; ENVIRONMENT; WEATHER; MECHANISMS
AB At 0300 UTC 9 September 2010, commercial aircraft traveling between Tokyo and Hawaii encountered regions of moderate and severe intensity turbulence at about 12-km elevation in or just above banded structures in the cirrus anvil associated with an oceanic cyclone located off the east coast of Japan. The generation mechanisms of the cirrus bands and turbulence are investigated using the Advanced Research Weather Research and Forecasting Model with five nested domains having a finest horizontal grid spacing of 370 m. The simulation reproduces the satellite-observed patterns of cloud brightness, including the bands, and suggests that synoptic-scale vertical shear within the anvil cloud layer and radiative effects, including long-wave cooling at cloud top and warming at cloud base, act together to produce banded structures within the southern edge of the cirrus cloud shield. The character of the bands within the nearly neutral or convectively unstable layer of the cirrus shield is similar to boundary layer rolls in that the vertical wind shear vectors are nearly parallel to the cirrus bands. The strong vertical shear aligned with the banded convection leads to flow deformations and mixing near the cloud top, resulting in localized moderate and severe turbulence. The estimated maximum value of the cube root of eddy dissipation rate within the bands is similar to 0.7 m(2/3) s(-1), consistent with severe turbulence levels experienced by large aircraft.
C1 [Kim, Jung-Hoon] Oak Ridge Associated Univ, NASA, Ames Res Ctr, Moffett Field, CA USA.
[Kim, Jung-Hoon; Chun, Hye-Yeong] Yonsei Univ, Dept Atmospher Sci, Seoul 120749, South Korea.
[Sharman, Robert D.; Trier, Stanley B.] Natl Ctr Atmospher Res, Boulder, CO 80307 USA.
RP Kim, JH (reprint author), NASA, Aviat Syst Div, Ames Res Ctr, Mail Code 210-10, Moffett Field, CA 94035 USA.
EM jung-hoon.kim@nasa.gov
FU Korean Meteorological Administration Research and Development Program
[CATER_2012-2011]; NOAA [NA-09NWS4670001]; Federal Aviation
Administration (FAA) Aviation Weather Research Program
FX This work was supported by the Korean Meteorological Administration
Research and Development Program under Grant CATER_2012-2011 (HYC and
JHK), NOAA Grant NA-09NWS4670001, and by the Federal Aviation
Administration (FAA) Aviation Weather Research Program (RDS and SBT).
The views expressed are those of the authors and do not necessarily
represent the official policy or position of the FAA. The authors thank
Melissa Thomas (Delta Air Lines) for a helpful review of a previous
version of the manuscript and for informative discussions concerning
real-time observations of the relation of cirrus bands to aviation
turbulence. The authors also appreciate the informative comments from
two anonymous reviewers, which helped clarify aspects of the paper.
NR 44
TC 5
Z9 5
U1 3
U2 6
PU AMER METEOROLOGICAL SOC
PI BOSTON
PA 45 BEACON ST, BOSTON, MA 02108-3693 USA
SN 0027-0644
EI 1520-0493
J9 MON WEATHER REV
JI Mon. Weather Rev.
PD AUG
PY 2014
VL 142
IS 8
BP 2794
EP 2813
DI 10.1175/MWR-D-14-00008.1
PG 20
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA AM6YZ
UT WOS:000340013200013
ER
PT J
AU Gregg, WW
Casey, NW
Rousseaux, CS
AF Gregg, Watson W.
Casey, Nancy W.
Rousseaux, Cecile S.
TI Sensitivity of simulated global ocean carbon flux estimates to forcing
by reanalysis products
SO OCEAN MODELLING
LA English
DT Article
DE Reanalysis; Ocean; Carbon; Fluxes; Models
ID ANTHROPOGENIC CARBON; GAS-EXCHANGE; WIND-SPEED; SYSTEM; MODEL;
VARIABILITY; PACIFIC; DUST
AB Reanalysis products from MERRA, NCEP2, NCEPI, and ECMWF were used to force an established ocean biogeochemical model to estimate air-sea carbon fluxes (FCO2) and partial pressure of carbon dioxide (pCO(2)) in the global oceans. Global air-sea carbon fluxes and pCO(2) were relatively insensitive to the choice of forcing reanalysis. All global FCO2 estimates from the model forced by the four different reanalyses were within 20% of in situ estimates (MERRA and NCEP1 were within 7%), and all models exhibited statistically significant positive correlations with in situ estimates across the 12 major oceanographic basins. Global pCO(2) estimates were within 1% of in situ estimates with ECMWF being the outlier at 0.6%. Basin correlations were similar to FCO2. There were, however, substantial departures among basin estimates from the different reanalysis forcings. The high latitudes and tropics had the largest ranges in estimated fluxes among the reanalyses. Regional pCO(2) differences among the reanalysis forcings were muted relative to the FCO2 results. No individual reanalysis was uniformly better or worse in the major oceanographic basins. The results provide information on the characterization of uncertainty in ocean carbon models due to choice of reanalysis forcing. Published by Elsevier Ltd. This is an open access article under the CC BY license (http://creativecommon-s.org/licenses/by/3.0/).
C1 [Gregg, Watson W.] NASA, Global Modeling & Assimilat Off, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Casey, Nancy W.] Sci Syst & Applicat Inc, Lanham, MD 20706 USA.
[Rousseaux, Cecile S.] NASA, Global Modeling & Assimilat Off, Goddard Space Flight Ctr, Univ Space Res Assoc, Greenbelt, MD 20771 USA.
RP Gregg, WW (reprint author), NASA, Global Modeling & Assimilat Off, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
EM watson.gregg@nasa.gov; nancy.casey@ssaihq.com;
cecile.s.rousseaux@nasa.gov
RI Rousseaux, Cecile/E-8811-2012
OI Rousseaux, Cecile/0000-0002-3022-2988
FU NASA
FX We thank the NASA/MERRA Project, the NOAA/NCEP Project and the ECMWF
Project for the data sets and public availability. We also thank the
Lamont-Doherty Earth Observatory for in situ pCO2 data and
flux estimates. We thank three anonymous reviewers for insights. This
work was supported by NASA Modeling and Analysis Program (MAP) and
Carbon Monitoring System (CMS) Programs.
NR 24
TC 2
Z9 2
U1 0
U2 7
PU ELSEVIER SCI LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND
SN 1463-5003
EI 1463-5011
J9 OCEAN MODEL
JI Ocean Model.
PD AUG
PY 2014
VL 80
BP 24
EP 35
DI 10.1016/j.ocemod.2014.05.002
PG 12
WC Meteorology & Atmospheric Sciences; Oceanography
SC Meteorology & Atmospheric Sciences; Oceanography
GA AN0YQ
UT WOS:000340310300003
ER
PT J
AU Elham, A
van Tooren, MJL
Sobieszczanski-Sobieski, J
AF Elham, Ali
van Tooren, Michel J. L.
Sobieszczanski-Sobieski, Jaroslaw
TI Bilevel Optimization Strategy for Aircraft Wing Design Using Parallel
Computing
SO AIAA JOURNAL
LA English
DT Article
ID SHAPE
AB A new bilevel optimization strategy for wing design is developed, in which the optimizations of the wing-planform and wing-airfoil shapes are decoupled from each other. The design of the wing-planform shape and the shape of the airfoils in several spanwise positions are considered as the goal of the optimization. In the new approach, the design problem is decomposed into a series of subproblems based on the design variables. The design variables defining the wing-planform shape are optimized in a top-level optimization, and the design variables defining the shape of airfoils in several spanwise positions are optimized in several sublevel optimizations. To take into account the influence of the airfoil shape in a specific spanwise position on the shape of the airfoils in other spanwise positions, a series of design variables are added to the design vector of the top-level optimization. The top-level optimizer is responsible for the consistency of the optimization. Using this approach, the number of design variables in the top-level optimization is reduced; the airfoils in several spanwise positions are optimized in parallel; and, instead of complex three-dimensional aerodynamic and structural solvers, much simpler and faster two-dimensional airfoil analysis tools can be used.
C1 [Elham, Ali] Delft Univ Technol, Fac Aerosp Engn, NL-2629 HS Delft, Netherlands.
[van Tooren, Michel J. L.] Univ S Carolina, Ronald E McNair Ctr Aerosp Innovat & Res, Columbia, SC 29201 USA.
[Sobieszczanski-Sobieski, Jaroslaw] NASA, Langley Res Ctr, Hampton, VA 23601 USA.
RP Elham, A (reprint author), Delft Univ Technol, Fac Aerosp Engn, Kluyverweg 1, NL-2629 HS Delft, Netherlands.
EM A.Elham@tudelft.nl; vantooren@cec.se.edu; ysobieskiy@gmail.com
NR 49
TC 2
Z9 2
U1 0
U2 9
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 AUG
PY 2014
VL 52
IS 8
BP 1770
EP 1783
DI 10.2514/1.J052696
PG 14
WC Engineering, Aerospace
SC Engineering
GA AM1XG
UT WOS:000339642000015
ER
PT J
AU Horvath, C
Envia, E
Podboy, GG
AF Horvath, Csaba
Envia, Edmane
Podboy, Gary G.
TI Limitations of Phased Array Beamforming in Open Rotor Noise Source
Imaging
SO AIAA JOURNAL
LA English
DT Article
C1 [Horvath, Csaba; Envia, Edmane; Podboy, Gary G.] NASA John H Glenn Res Ctr Lewis Field, Cleveland, OH 44135 USA.
RP Horvath, C (reprint author), Budapest Univ Technol & Econ, Budapest, Hungary.
EM horvath@ara.bme.hu
FU Environmentally Responsible Aviation Project of the NASA Integrated
Systems Research Program; Fixed Wing Project of the NASA Fundamental
Aeronautics Program; Hungarian Fund for Science and Research [K 83807];
relates to the scientific program of the projects "Development of
quality-oriented and harmonized R + D + 1 strategy and the functional
model at BME" [TAMOP-4.2.1/B-09/1/KMR-2010-0002]; "Talent care and
cultivation in the scientific workshops of BME"
[TAMOP-4.2.2/B-10/1-2010-0009]
FX This testing and research was funded by the Environmentally Responsible
Aviation Project of the NASA Integrated Systems Research Program and the
Fixed Wing Project of the NASA Fundamental Aeronautics Program. A
portion of the study and the publication of the work was supported by
the Hungarian Fund for Science and Research under Contract No. K 83807
and relates to the scientific program of the projects "Development of
quality-oriented and harmonized R + D + 1 strategy and the functional
model at BME" and "Talent care and cultivation in the scientific
workshops of BME" under Grants No. TAMOP-4.2.1/B-09/1/KMR-2010-0002 and
No. TAMOP-4.2.2/B-10/1-2010-0009, respectively.
NR 16
TC 9
Z9 9
U1 1
U2 2
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 AUG
PY 2014
VL 52
IS 8
BP 1810
EP 1817
DI 10.2514/1.J052952
PG 8
WC Engineering, Aerospace
SC Engineering
GA AM1XG
UT WOS:000339642000021
ER
PT J
AU Borkowski, KJ
Reynolds, SP
Green, DA
Hwang, U
Petre, R
Krishnamurthy, K
Willett, R
AF Borkowski, Kazimierz J.
Reynolds, Stephen P.
Green, David A.
Hwang, Una
Petre, Robert
Krishnamurthy, Kalyani
Willett, Rebecca
TI NONUNIFORM EXPANSION OF THE YOUNGEST GALACTIC SUPERNOVA REMNANT G1.9+0.3
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE ISM: individual objects (G1.9+0.3); ISM: supernova remnants; X-rays: ISM
ID HIGH-VELOCITY FEATURES; IA SUPERNOVAE; EXPLOSION MECHANISM; MODELS;
EJECTA; CONSTRAINTS
AB We report measurements of the X-ray expansion of the youngest Galactic supernova remnant, G1.9+0.3, using Chandra observations in 2007, 2009, and 2011. The measured rates strongly deviate from uniform expansion, decreasing radially by about 60% along the X-ray bright SE-NW axis from 0.84% +/- 0.06% yr(-1) to 0.52% +/- 0.03% yr(-1). This corresponds to undecelerated ages of 120-190 yr, confirming the young age of G1.9+0.3 and implying a significant deceleration of the blast wave. The synchrotron-dominated X-ray emission brightens at a rate of 1.9% +/- 0.4% yr(-1). We identify bright outer and inner rims with the blast wave and reverse shock, respectively. Sharp density gradients in either the ejecta or ambient medium are required to produce the sudden deceleration of the reverse shock or the blast wave implied by the large spread in expansion ages. The blast wave could have been decelerated recently by an encounter with a modest density discontinuity in the ambient medium, such as may be found at a wind termination shock, requiring strong mass loss in the progenitor. Alternatively, the reverse shock might have encountered an order-of-magnitude density discontinuity within the ejecta, such as may be found in pulsating delayed-detonation Type Ia models. We demonstrate that the blast wave is much more decelerated than the reverse shock in these models for remnants at ages similar to G1.9+0.3. Similar effects may also be produced by dense shells possibly associated with high-velocity features in Type Ia spectra. Accounting for the asymmetry of G1.9+0.3 will require more realistic three-dimensional Type Ia models.
C1 [Borkowski, Kazimierz J.; Reynolds, Stephen P.] N Carolina State Univ, Dept Phys, Raleigh, NC 27695 USA.
[Green, David A.] Univ Cambridge, Cavendish Lab, Cambridge CB3 0HE, England.
[Hwang, Una] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Petre, Robert] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Krishnamurthy, Kalyani] Duke Univ, Dept Elect & Comp Engn, Durham, NC 27708 USA.
[Willett, Rebecca] Univ Wisconsin, Dept Elect & Comp Engn, Madison, WI 53706 USA.
RP Borkowski, KJ (reprint author), N Carolina State Univ, Dept Phys, Raleigh, NC 27695 USA.
EM kborkow@unity.ncsu.edu
RI Green, David/E-9609-2010;
OI Green, David/0000-0003-3189-9998; Willett, Rebecca/0000-0002-8109-7582
FU NASA through Chandra General Observer Program [SAO G01-12098A, SAO
G01-12098B]
FX This work was supported by NASA through Chandra General Observer Program
grants SAO G01-12098A and B.
NR 24
TC 4
Z9 4
U1 0
U2 0
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 AUG 1
PY 2014
VL 790
IS 2
AR L18
DI 10.1088/2041-8205/790/2/L18
PG 6
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AM5KO
UT WOS:000339897100004
ER
PT J
AU Piro, L
Troja, E
Gendre, B
Ghisellini, G
Ricci, R
Bannister, K
Fiore, F
Kidd, LA
Piranomonte, S
Wieringa, MH
AF Piro, Luigi
Troja, Eleonora
Gendre, Bruce
Ghisellini, Gabriele
Ricci, Roberto
Bannister, Keith
Fiore, Fabrizio
Kidd, Lauren A.
Piranomonte, Silvia
Wieringa, Mark H.
TI A HOT COCOON IN THE ULTRALONG GRB 130925A: HINTS OF A POPIII-LIKE
PROGENITOR IN A LOW-DENSITY WIND ENVIRONMENT
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE gamma-ray burst: individual (GRB130925A); stars: Population III
ID GAMMA-RAY BURSTS; POPULATION-III STARS; MASSIVE STARS; 1ST STARS; SWIFT;
JETS; AFTERGLOWS; SUPERNOVA; EMISSION; CONNECTION
AB GRB 130925A is a peculiar event characterized by an extremely long gamma-ray duration (approximate to 7 ks), as well as dramatic flaring in the X-rays for approximate to 20 ks. After this period, its X-ray afterglow shows an atypical soft spectrum with photon index Gamma similar to 4, as observed by Swift and Chandra, until approximate to 10(7) s, when XMM-Newton observations uncover a harder spectral shape with Gamma similar to 2.5, commonly observed in gamma-ray burst (GRB) afterglows. We find that two distinct emission components are needed to explain the X-ray observations: a thermal component, which dominates the X-ray emission for several weeks, and a non-thermal component, consistent with a typical afterglow. A forward shock model well describes the broadband (from radio to X-rays) afterglow spectrum at various epochs. It requires an ambient medium with a very low-density wind profile, consistent with that expected from a low-metallicity blue supergiant (BSG). The thermal component has a remarkably constant size and a total energy consistent with those expected by a hot cocoon surrounding the relativistic jet. We argue that the features observed in this GRB (its ultralong duration, the thermal cocoon, and the low-density wind environment) are associated with a low metallicity BSG progenitor and, thus, should characterize the class of ultralong GRBs.
C1 [Piro, Luigi] INAF Ist Astrofis Planetol Spaziali, I-00133 Rome, Italy.
[Troja, Eleonora; Kidd, Lauren A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Gendre, Bruce] ARTEMIS, UMR 7250, F-06304 Nice 4, France.
[Ghisellini, Gabriele] INAF Osservatorio Astron Brera, I-23807 Merate, LC, Italy.
[Ricci, Roberto] INAF Ist Radioastron, I-40129 Bologna, Italy.
[Bannister, Keith] CSIRO Astron & Space Sci, Marsfield, NSW 2122, Australia.
[Fiore, Fabrizio; Piranomonte, Silvia] INAF Osservatorio Astron Roma, I-00040 Monte Porzio Catone, RM, Italy.
[Wieringa, Mark H.] CSIRO Astron & Space Sci, Narrabri, NSW 2390, Australia.
RP Piro, L (reprint author), INAF Ist Astrofis Planetol Spaziali, Via Fosso Cavaliere 100, I-00133 Rome, Italy.
OI Piranomonte, Silvia/0000-0002-8875-5453; Bannister,
Keith/0000-0003-2149-0363; Ghisellini, Gabriele/0000-0002-0037-1974;
Gendre, Bruce/0000-0002-9077-2025; Fiore, Fabrizio/0000-0002-4031-4157
NR 42
TC 20
Z9 20
U1 1
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 AUG 1
PY 2014
VL 790
IS 2
AR L15
DI 10.1088/2041-8205/790/2/L15
PG 5
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AM5KO
UT WOS:000339897100001
ER
PT J
AU Tremblay, GR
Gladders, MD
Baum, SA
O'Dea, CP
Bayliss, MB
Cooke, KC
Dahle, H
Davis, TA
Florian, M
Rigby, JR
Sharon, K
Soto, E
Wuyts, E
AF Tremblay, Grant R.
Gladders, Michael D.
Baum, Stefi A.
O'Dea, Christopher P.
Bayliss, Matthew B.
Cooke, Kevin C.
Dahle, Hakon
Davis, Timothy A.
Florian, Michael
Rigby, Jane R.
Sharon, Keren
Soto, Emmaris
Wuyts, Eva
TI A 30 kpc CHAIN OF "BEADS ON A STRING" STAR FORMATION BETWEEN TWO MERGING
EARLY TYPE GALAXIES IN THE CORE OF A STRONG-LENSING GALAXY CLUSTER
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE galaxies: clusters: general; galaxies: clusters: individual (SDSS
J1531+3414); galaxies; interactions; galaxies: star formation;
gravitational lensing: strong
ID COLOR-MAGNITUDE RELATIONS; GIANT ARCS; PROJECT; CONSTRAINTS; EVOLUTION;
ORIGIN; SCALES; GAS; LAW
AB New Hubble Space Telescope ultraviolet and optical imaging of the strong-lensing galaxy cluster SDSS J1531+3414 (z = 0.335) reveals two centrally dominant elliptical galaxies participating in an ongoing major merger. The interaction is at least somewhat rich in cool gas, as the merger is associated with a complex network of 19 massive superclusters of young stars (or small tidal dwarf galaxies) separated by similar to 1 kpc in projection from one another, combining to an estimated total star formation rate of similar to 5 M-circle dot yr(-1). The resolved young stellar superclusters are threaded by narrow Ha, [O-II], and blue excess filaments arranged in a network spanning similar to 27 kpc across the two merging galaxies. This morphology is strongly reminiscent of the well-known " beads on a string" mode of star formation observed on kiloparsecscales in the arms of spiral galaxies, resonance rings, and in tidal tails between interacting galaxies. Nevertheless, the arrangement of this star formation relative to the nuclei of the two galaxies is difficult to interpret in a dynamical sense, as no known " beads on a string" systems associated with kiloparsec-scale tidal interactions exhibit such lopsided morphology relative to the merger participants. In this Letter, we present the images and follow-up spectroscopy and discuss possible physical interpretations for the unique arrangement of the young stellar clusters. While we suggest that this morphology is likely to be dynamically short-lived, a more quantitative understanding awaits necessary multiwavelength follow-up, including optical integral field spectroscopy, ALMA submillimeter interferometry, and Chandra X-ray imaging.
C1 [Tremblay, Grant R.; Davis, Timothy A.] European So Observ, D-85748 Garching, Germany.
[Gladders, Michael D.; Florian, Michael] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA.
[Gladders, Michael D.; Florian, Michael] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA.
[Baum, Stefi A.; O'Dea, Christopher P.; Cooke, Kevin C.] Rochester Inst Technol, Chester F Carlson Ctr Imaging Sci, Rochester, NY 14623 USA.
[Baum, Stefi A.; O'Dea, Christopher P.; Cooke, Kevin C.] Rochester Inst Technol, Sch Phys & Astron, Rochester, NY 14623 USA.
[Bayliss, Matthew B.] Harvard Univ, Dept Phys, Cambridge, MA 02138 USA.
[Bayliss, Matthew B.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Dahle, Hakon] Univ Oslo, Inst Theoret Astrophys, N-0315 Oslo, Norway.
[Rigby, Jane R.] NASA, Goddard Space Flight Ctr, Observat Cosmol Lab, Greenbelt, MD 20771 USA.
[Sharon, Keren] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA.
[Soto, Emmaris] Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA.
[Wuyts, Eva] Max Planck Inst Extraterr Phys, D-85741 Garching, Germany.
RP Tremblay, GR (reprint author), European So Observ, Karl Schwarzschild Str 2, D-85748 Garching, Germany.
EM grant.tremblay@eso.org
RI Rigby, Jane/D-4588-2012;
OI Rigby, Jane/0000-0002-7627-6551; Davis, Timothy/0000-0003-4932-9379;
Cooke, Kevin/0000-0002-2200-9845; Tremblay, Grant/0000-0002-5445-5401;
Florian, Michael/0000-0001-5097-6755
FU European Community [229517]; NASA [HST-GO-13003]; Association of
Universities for Research in Astronomy, Inc., under NASA [NAS5-26555];
Alfred P. Sloan Foundation; SDSS; Participating Institutions; 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 Professors Francoise Combes, Eric Emsellem, and Tim de Zeeuw
for thoughtful discussions. We also thank the anonymous referee whose
feedback improved this work. G. R. T. and T. A. D. acknowledge support
from a European Southern Observatory (ESO) Fellowship partially funded
by the European Community's Seventh Framework Programme
(/FP7/2007-2013/) under grant agreement No. 229517. Support for program
number HST-GO-13003 was provided by NASA through a grant from the Space
Telescope Science Institute, which is operated by the Association of
Universities for Research in Astronomy, Inc., under NASA contract
NAS5-26555. This Letter is based on observations by the NASA/ESA Hubble
Space Telescope, obtained at the Space Telescope Science Institute. We
also present results from the Nordic Optical Telescope, operated by the
Nordic Optical Telescope Scientific Association at the Observatorio del
Roque de los Muchachos, La Palma, Spain, of the Instituto de Astrofisica
de Canarias. 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. The SDSS Web site is http://www.sdss.org/.
NR 35
TC 5
Z9 5
U1 0
U2 1
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 AUG 1
PY 2014
VL 790
IS 2
AR L26
DI 10.1088/2041-8205/790/2/L26
PG 6
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AM5KO
UT WOS:000339897100012
ER
PT J
AU Xiao, H
Mechoso, CR
Sun, RY
Han, J
Pan, HL
Park, S
Hannay, C
Bretherton, C
Teixeira, J
AF Xiao, Heng
Mechoso, C. Roberto
Sun, Ruiyu
Han, Jongil
Pan, Hua-Lu
Park, Sungsu
Hannay, Cecile
Bretherton, Chris
Teixeira, Joao
TI Diagnosis of the marine low cloud simulation in the NCAR community earth
system model (CESM) and the NCEP global forecast system (GFS)-modular
ocean model v4 (MOM4) coupled model
SO CLIMATE DYNAMICS
LA English
DT Article
DE Marine low clouds; Stratocumulus; Shallow cumulus; Climate modeling;
CESM; GFS; Parameterization; Stratocumulus to cumulus transition
ID BOUNDARY-LAYER CLOUDS; GENERAL-CIRCULATION MODELS; ATMOSPHERE MODEL;
SOUTHEAST PACIFIC; SEASONAL CYCLE; PART I; CLIMATE SIMULATIONS; CUMULUS
CONVECTION; VERTICAL DIFFUSION; TROPICAL PACIFIC
AB We present a diagnostic analysis of the marine low cloud climatology simulated by two state-of-the-art coupled atmosphere-ocean models: the National Center for Atmospheric Research community earth system model version 1 (CESM1) and the National Center for Environmental Predictions global forecasting system-modular ocean model version 4 (GFS-MOM4) coupled model. In the CESM1, the coastal stratocumulus (Sc)-topped planetary boundary layers (PBLs) in the subtropical Eastern Pacific are well-simulated but the climatological transition from Sc to shallow cumulus (Cu) is too abrupt and occurs too close to the coast. By contrast, in the GFS-MOM4 the coastal Sc amount and PBL depth are severely underestimated while the transition from Sc to shallow Cu is "delayed" and offshore Sc cover is too extensive in the subtropical Eastern Pacific. We discuss the possible connections between these differences in the simulations and differences in the parameterizations of shallow convection and boundary layer turbulence in the two models.
C1 [Xiao, Heng; Mechoso, C. Roberto] Univ Calif Los Angeles, Dept Atmospher & Ocean Sci, Los Angeles, CA USA.
[Sun, Ruiyu; Han, Jongil; Pan, Hua-Lu] NOAA, Natl Ctr Environm Predict, Silver Spring, MD USA.
[Park, Sungsu; Hannay, Cecile] Natl Ctr Atmospher Res, Boulder, CO 80307 USA.
[Bretherton, Chris] Univ Washington, Dept Atmospher Sci, Seattle, WA 98195 USA.
[Teixeira, Joao] CALTECH, Jet Prop Lab, Pasadena, CA USA.
RP Xiao, H (reprint author), Pacific NW Natl Lab, Atmospher Sci & Global Change Div, POB 999, Richland, WA 99352 USA.
EM Heng.Xiao@pnnl.gov
FU NOAA MAPP/CPO; U.S. DOE OBER [KP/501021/58166]; US Department of Energy
[DE-AC05-76RL01830]; National Science Foundation
FX This work is supported by the NOAA MAPP/CPO program as part of the Sc-Cu
Climate Process Team through grants to UCLA, NCAR, NCEP, UW and JPL. HX
was supported by U.S. DOE OBER grant KP/501021/58166 at PNNL. We also
acknowledge helpful suggestions from all four anonymous reviewers.
Pacific Northwest National Laboratory is operated by Battelle Memorial
Institute for the US Department of Energy under Contract No.
DE-AC05-76RL01830. The National Center for Atmospheric Research is
sponsored by the National Science Foundation.
NR 69
TC 3
Z9 3
U1 0
U2 11
PU SPRINGER
PI NEW YORK
PA 233 SPRING ST, NEW YORK, NY 10013 USA
SN 0930-7575
EI 1432-0894
J9 CLIM DYNAM
JI Clim. Dyn.
PD AUG
PY 2014
VL 43
IS 3-4
BP 737
EP 752
DI 10.1007/s00382-014-2067-y
PG 16
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA AM5LG
UT WOS:000339899500010
ER
PT J
AU Minson, SE
Simons, M
Beck, JL
Ortega, F
Jiang, J
Owen, SE
Moore, AW
Inbal, A
Sladen, A
AF Minson, S. E.
Simons, M.
Beck, J. L.
Ortega, F.
Jiang, J.
Owen, S. E.
Moore, A. W.
Inbal, A.
Sladen, A.
TI Bayesian inversion for finite fault earthquake source models - II: the
2011 great Tohoku-oki, Japan earthquake
SO GEOPHYSICAL JOURNAL INTERNATIONAL
LA English
DT Article
DE Inverse theory; Probability distributions; Earthquake source
observations; Computational seismology
ID WAVE-FORM INVERSION; NORTHEASTERN JAPAN; STRUCTURAL CHARACTERISTICS;
NORTHERN HONSHU; PACIFIC COAST; TRENCH AXIS; ARC REGION; SLIP; RUPTURE;
REFLECTION
AB We present a fully Bayesian inversion of kinematic rupture parameters for the 2011 M(w)9 Tohoku-oki, Japan earthquake. Albeit computationally expensive, this approach to kinematic source modelling has the advantage of producing an ensemble of slip models that are consistent with physical a priori constraints, realistic data uncertainties, and realistic but simplistic uncertainties in the physics of the kinematic forward model, all without being biased by non-physical regularization constraints. Combining 1 Hz kinematic GPS, static GPS offsets, seafloor geodesy and near-field and far-field tsunami data into a massively parallel Monte Carlo simulation, we construct an ensemble of samples of the posterior probability density function describing the evolution of fault rupture. We find that most of the slip is concentrated in a depth range of 10-20 km from the trench, and that slip decreases towards the trench with significant displacements at the toe of wedge occurring in just a small region. Estimates of static stress drop and rupture velocity are ambiguous. Due to the spatial compactness of the fault rupture, the duration of the entire rupture was less than approximately 150 s.
C1 [Minson, S. E.; Simons, M.; Ortega, F.; Jiang, J.; Inbal, A.] CALTECH, Div Geol & Planetary Sci, Seismol Lab, Pasadena, CA 91125 USA.
[Beck, J. L.] CALTECH, Div Engn & Appl Sci, Pasadena, CA 91125 USA.
[Owen, S. E.; Moore, A. W.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Sladen, A.] Univ Nice, CNRS UMR 7329, Geoazur, Observ Cote Azur,IRD,UPMC, Valbonne, France.
RP Minson, SE (reprint author), CALTECH, Div Geol & Planetary Sci, Seismol Lab, Pasadena, CA 91125 USA.
EM minson@gps.caltech.edu
RI Ortega-Culaciati, Francisco Hernan/A-2587-2014; Sladen,
Anthony/A-2532-2017;
OI Ortega-Culaciati, Francisco Hernan/0000-0002-2983-8646; Sladen,
Anthony/0000-0003-4126-0020; Jiang, Junle/0000-0002-8796-5846; Simons,
Mark/0000-0003-1412-6395
FU National Science Foundation [EAR-0941374]
FX The CATMIP MCMC simulations were executed on NASA's Pleiades
supercomputer. This work is supported by the National Science Foundation
through grant number EAR-0941374 and is Caltech Seismological Laboratory
contribution 10087.
NR 52
TC 18
Z9 18
U1 2
U2 21
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 AUG
PY 2014
VL 198
IS 2
BP 922
EP 940
DI 10.1093/gji/ggu170
PG 19
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA AM2YN
UT WOS:000339717700018
ER
PT J
AU Mukhanov, O
Johnson, M
Kleinsasser, A
AF Mukhanov, Oleg
Johnson, Mark
Kleinsasser, Alan
TI SPECIAL ISSUE ON THE 2013 INTERNATIONAL SUPERCONDUCTIVE ELECTRONICS
CONFERENCE (ISEC)
SO IEEE TRANSACTIONS ON APPLIED SUPERCONDUCTIVITY
LA English
DT Editorial Material
C1 [Mukhanov, Oleg] Hypres Inc, Elmsford, NY 10523 USA.
[Johnson, Mark] D Wave Syst Inc, Burnaby, BC V5C 4M9, Canada.
[Kleinsasser, Alan] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Mukhanov, O (reprint author), Hypres Inc, 175 Clearbrook Rd, Elmsford, NY 10523 USA.
NR 0
TC 0
Z9 0
U1 0
U2 3
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 1051-8223
EI 1558-2515
J9 IEEE T APPL SUPERCON
JI IEEE Trans. Appl. Supercond.
PD AUG
PY 2014
VL 24
IS 4
AR 0002101
DI 10.1109/TASC.2014.2332671
PG 1
WC Engineering, Electrical & Electronic; Physics, Applied
SC Engineering; Physics
GA AM7ZZ
UT WOS:000340089200001
ER
PT J
AU Wang, H
Long, L
Kumar, A
Wang, WQ
Schemm, JKE
Zhao, M
Vecchi, GA
Larow, TE
Lim, YK
Schubert, SD
Shaevitz, DA
Camargo, SJ
Henderson, N
Kim, D
Jonas, JA
Walsh, KJE
AF Wang, Hui
Long, Lindsey
Kumar, Arun
Wang, Wanqiu
Schemm, Jae-Kyung E.
Zhao, Ming
Vecchi, Gabriel A.
Larow, Timothy E.
Lim, Young-Kwon
Schubert, Siegfried D.
Shaevitz, Daniel A.
Camargo, Suzana J.
Henderson, Naomi
Kim, Daehyun
Jonas, Jeffrey A.
Walsh, Kevin J. E.
TI How Well Do Global Climate Models Simulate the Variability of Atlantic
Tropical Cyclones Associated with ENSO?
SO JOURNAL OF CLIMATE
LA English
DT Article
ID GENERAL-CIRCULATION MODELS; SEA-SURFACE TEMPERATURE; NORTH-ATLANTIC;
EL-NINO; HURRICANE ACTIVITY; CMIP5 MODELS; FORECAST; GCM; PRECIPITATION;
OSCILLATION
AB The variability of Atlantic tropical cyclones (TCs) associated with El Nino-Southern Oscillation (ENSO) in model simulations is assessed and compared with observations. The model experiments are 28-yr simulations forced with the observed sea surface temperature from 1982 to 2009. The simulations were coordinated by the U.S. Climate Variability and Predictability Research Program (CLIVAR) Hurricane Working Group and conducted with five global climate models (GCMs) with a total of 16 ensemble members. The model performance is evaluated based on both individual model ensemble means and multimodel ensemble mean. The latter has the highest anomaly correlation (0.86) for the interannual variability of TCs. Previous observational studies show a strong association between ENSO and Atlantic TC activity, as well as distinctions during eastern Pacific (EP) and central Pacific (CP) El Nino events. The analysis of track density and TC origin indicates that each model has different mean biases. Overall, the GCMs simulate the variability of Atlantic TCs well with weaker activity during EP El Nino and stronger activity during La Nina. For CP El Nino, there is a slight increase in the number of TCs as compared with EP El Nino. However, the spatial distribution of track density and TC origin is less consistent among the models. Particularly, there is no indication of increasing TC activity over the U.S. southeast coastal region during CP El Nino as in observations. The difference between the models and observations is likely due to the bias of the models in response to the shift of tropical heating associated with CP El Nino, as well as the model bias in the mean circulation.
C1 [Wang, Hui; Long, Lindsey; Kumar, Arun; Wang, Wanqiu; Schemm, Jae-Kyung E.] NOAA, NWS, NCEP, Climate Predict Ctr, College Pk, MD 20740 USA.
[Wang, Hui; Long, Lindsey] Innovim, Greenbelt, MD USA.
[Zhao, Ming; Vecchi, Gabriel A.] NOAA, Geophys Fluid Dynam Lab, Princeton, NJ USA.
[Larow, Timothy E.] Florida State Univ, Ctr Ocean Atmospher Predict Studies, Tallahassee, FL 32306 USA.
[Lim, Young-Kwon; Schubert, Siegfried D.] NASA, Goddard Space Flight Ctr, Global Modeling & Assimilat Off, Greenbelt, MD 20771 USA.
[Lim, Young-Kwon] IM Syst Grp, Goddard Earth Sci Technol & Res, Greenbelt, MD USA.
[Shaevitz, Daniel A.] Columbia Univ, Dept Appl Phys & Appl Math, New York, NY USA.
[Camargo, Suzana J.; Henderson, Naomi; Kim, Daehyun] Columbia Univ, Lamont Doherty Earth Observ, Palisades, NY USA.
[Jonas, Jeffrey A.] Columbia Univ, Ctr Climate Syst Res, New York, NY USA.
[Jonas, Jeffrey A.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
[Walsh, Kevin J. E.] Univ Melbourne, Sch Earth Sci, Parkville, Vic 3052, Australia.
RP Wang, H (reprint author), NOAA, Climate Predict Ctr, NCWCP, 5830 Univ Res Court, College Pk, MD 20740 USA.
EM hui.wang@noaa.gov
RI Camargo, Suzana/C-6106-2009; Vecchi, Gabriel/A-2413-2008; Zhao,
Ming/C-6928-2014;
OI Camargo, Suzana/0000-0002-0802-5160; Vecchi,
Gabriel/0000-0002-5085-224X; Walsh, Kevin/0000-0002-1860-510X
FU U.S. CLIVAR
FX This work was carried out as part of a Hurricane Working Group activity
supported by the U.S. CLIVAR. The authors thank the Lamont-Doherty Earth
Observatory of Columbia University for archiving model data and making
them accessible online. The authors also thank Prof. Kerry A. Emanuel,
Dr. Christopher W. Landsea, Mr. Bill Mohan, an anonymous reviewer, and
the editor for their insightful and constructive comments and
suggestions.
NR 50
TC 11
Z9 11
U1 4
U2 30
PU AMER METEOROLOGICAL SOC
PI BOSTON
PA 45 BEACON ST, BOSTON, MA 02108-3693 USA
SN 0894-8755
EI 1520-0442
J9 J CLIMATE
JI J. Clim.
PD AUG 1
PY 2014
VL 27
IS 15
BP 5673
EP 5692
DI 10.1175/JCLI-D-13-00625.1
PG 20
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA AM2SY
UT WOS:000339702300001
ER
PT J
AU Xia, YL
Ek, MB
Mocko, D
Peters-Lidard, CD
Sheffield, J
Dong, JR
Wood, EF
AF Xia, Youlong
Ek, Michael B.
Mocko, David
Peters-Lidard, Christa D.
Sheffield, Justin
Dong, Jiarui
Wood, Eric F.
TI Uncertainties, Correlations, and Optimal Blends of Drought Indices from
the NLDAS Multiple Land Surface Model Ensemble
SO JOURNAL OF HYDROMETEOROLOGY
LA English
DT Article
ID ASSIMILATION SYSTEM NLDAS; UNITED-STATES; 20TH-CENTURY DROUGHT; MONITOR
AB This study analyzed uncertainties and correlations over the United States among four ensemble-mean North American Land Data Assimilation System (NLDAS) percentile-based drought indices derived from monthly mean evapotranspiration ET, total runoff Q, top 1-m soil moisture SM1, and total column soil moisture SMT. The results show that the uncertainty is smallest for SM1, largest for SMT, and moderate for ET and Q. The strongest correlation is between SM1 and SMT, and the weakest correlation is between ET and Q. The correlation between ET and SM1 (SMT) is strongest in arid-semiarid regions, and the correlation between Q and SM1 (SMT) is strongest in more humid regions in the Pacific Northwest and the Southeast. Drought frequency analysis shows that SM1 has the most frequent drought occurrence, followed by SMT, Q, and ET. The study compared the NLDAS drought indices (a research product) with the U.S. Drought Monitor (USDM; an operational product) in terms of drought area percentage derived from each product. It proposes an optimal blend of NLDAS drought indices by searching for weights for each index that minimizes the RMSE between NLDAS and USDM drought area percentage for a 10-yr period (2000-09) with a cross validation. It reconstructed a 30-yr (1980-2009) Objective Blended NLDAS Drought Index (OBNDI) and monthly drought percentage. Overall, the OBNDI performs the best with the smallest RMSE, followed by SM1 and SMT. It should be noted that the contribution to OBNDI from different variables varies with region. So a single formula is probably not the best representation of a blended index. The representation of a blended index using the multiple formulas will be addressed in a future study.
C1 [Xia, Youlong; Dong, Jiarui] Environm Modeling Ctr, IMSG, College Pk, MD 20740 USA.
[Xia, Youlong; Ek, Michael B.; Dong, Jiarui] NOAA, NCEP, EMC, IMSG, College Pk, MD 20740 USA.
[Mocko, David; Peters-Lidard, Christa D.] NASA, Goddard Space Flight Ctr, Hydrol Sci Lab, Greenbelt, MD 20771 USA.
[Mocko, David] SAIC, Greenbelt, MD USA.
[Sheffield, Justin; Wood, Eric F.] Princeton Univ, Dept Environm & Civil Engn, Princeton, NJ 08544 USA.
RP Xia, YL (reprint author), NOAA, NCEP, EMC, IMSG, 5830 Univ Res Court, College Pk, MD 20740 USA.
EM youlong.xia@noaa.gov
RI Peters-Lidard, Christa/E-1429-2012
OI Peters-Lidard, Christa/0000-0003-1255-2876
FU NOAA Climate Program Office's Modeling, Analysis, Prediction, and
Projection (MAPP) program
FX This study is sponsored by the NOAA Climate Program Office's Modeling,
Analysis, Prediction, and Projection (MAPP) program. We thank Dr.
Kingtse Mo from Climate Prediction Center, who provided SPI3 and SPI6
derived from CPC gauge precipitation data used in NLDAS-2. Y.X. thanks
Dr. Weiyu Yang from EMC and three anonymous reviewers, whose comments
and suggestions greatly improved the quality of this manuscript.
NR 27
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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 AUG
PY 2014
VL 15
IS 4
BP 1636
EP 1650
DI 10.1175/JHM-D-13-058.1
PG 15
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA AM2QX
UT WOS:000339697000020
ER
PT J
AU Zhou, T
Nijssen, B
Huffman, GJ
Lettenmaier, DP
AF Zhou, Tian
Nijssen, Bart
Huffman, George J.
Lettenmaier, Dennis P.
TI Evaluation of Real-Time Satellite Precipitation Data for Global Drought
Monitoring
SO JOURNAL OF HYDROMETEOROLOGY
LA English
DT Article
ID CONTERMINOUS UNITED-STATES; ANALYSIS TMPA; TRENDS; RAINFALL; SCALES
AB The Tropical Rainfall Measuring Mission (TRMM) Multi-satellite Precipitation Analysis (TMPA) near-real-time (RT) data are considered less accurate than the TMPA research quality (RP) data because of the simplified data processing algorithm and the lack of gauge adjustments. However, for near-real-time hydrological applications, such as drought nowcasting, the RT data must play a key role given latency considerations and consistency is essential with products like RP, which have a long-term climatology. The authors used a bivariate test to examine the consistency between the monthly RT and RP precipitation estimates for 12 yr (2000-12) and found that, for over 75% of land cells globally, RT and RP were statistically consistent at 0.05 significance level. The inconsistent grid cells are spatially clustered in western North America, northern South America, central Africa, and most of Australia. The authors also show that RT generally increases with time relative to RP in northern South America and western Australia, while in western North America and eastern Australia, RT decreases relative to RP. In other areas such as the eastern part of North America, Eurasia, and southern part of the South America, the RT data are statistically consistent with the RP data and are appropriate for global- or macroscale hydrological applications.
C1 [Zhou, Tian; Nijssen, Bart; Lettenmaier, Dennis P.] Univ Washington, Dept Civil & Environm Engn, Seattle, WA 98195 USA.
[Huffman, George J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Lettenmaier, DP (reprint author), Univ Washington, Dept Civil & Environm Engn, 202D Wilson Ceram Lab,Box 352700, Seattle, WA 98195 USA.
EM dennisl@uw.edu
RI Zhou, Tian/F-8659-2015; Nijssen, Bart/B-1013-2012; Huffman,
George/F-4494-2014
OI Zhou, Tian/0000-0003-1582-4005; Nijssen, Bart/0000-0002-4062-0322;
Huffman, George/0000-0003-3858-8308
FU NASA [NNX10AG87G]
FX This study was supported by NASA Grant NNX10AG87G to the University of
Washington. The authors thank David Bolvin for thoughtful comments,
Huilin Gao for data sharing, and Faisal Hossain for his suggestions on
an earlier draft of the manuscript.
NR 25
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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 AUG
PY 2014
VL 15
IS 4
BP 1651
EP 1660
DI 10.1175/JHM-D-13-0128.1
PG 10
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA AM2QX
UT WOS:000339697000021
ER
PT J
AU Kitching, TD
Heavens, AF
Alsing, J
Erben, T
Heymans, C
Hildebrandt, H
Hoekstra, H
Jaffe, A
Kiessling, A
Mellier, Y
Miller, L
van Waerbeke, L
Benjamin, J
Coupon, J
Fu, L
Hudson, MJ
Kilbinger, M
Kuijken, K
Rowe, BTP
Schrabback, T
Semboloni, E
Velander, M
AF Kitching, T. D.
Heavens, A. F.
Alsing, J.
Erben, T.
Heymans, C.
Hildebrandt, H.
Hoekstra, H.
Jaffe, A.
Kiessling, A.
Mellier, Y.
Miller, L.
van Waerbeke, L.
Benjamin, J.
Coupon, J.
Fu, L.
Hudson, M. J.
Kilbinger, M.
Kuijken, K.
Rowe, B. T. P.
Schrabback, T.
Semboloni, E.
Velander, M.
TI 3D cosmic shear: cosmology from CFHTLenS
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE gravitational lensing: weak; cosmological parameters
ID WEAK-LENSING SURVEYS; GALAXY SHAPE MEASUREMENT; MATTER POWER SPECTRUM;
HUBBLE-SPACE-TELESCOPE; DARK ENERGY; INTRINSIC ALIGNMENTS; PRECISION
COSMOLOGY; COVARIANCE-MATRIX; HALO MODEL; CONSTRAINTS
AB This paper presents the first application of 3D cosmic shear to a wide-field weak lensing survey. 3D cosmic shear is a technique that analyses weak lensing in three dimensions using a spherical harmonic approach, and does not bin data in the redshift direction. This is applied to CFHTLenS, a 154 square degree imaging survey with a median redshift of 0.7 and an effective number density of 11 galaxies per square arcminute usable for weak lensing. To account for survey masks we apply a 3D pseudo-C-a"" approach on weak lensing data, and to avoid uncertainties in the highly non-linear regime, we separately analyse radial wavenumbers k a parts per thousand currency sign 1.5 and 5.0 h Mpc(-1), and angular wavenumbers a"" a parts per thousand 400-5000. We show how one can recover 2D and tomographic power spectra from the full 3D cosmic shear power spectra and present a measurement of the 2D cosmic shear power spectrum, and measurements of a set of 2-bin and 6-bin cosmic shear tomographic power spectra; in doing so we find that using the 3D power in the calculation of such 2D and tomographic power spectra from data naturally accounts for a minimum scale in the matter power spectrum. We use 3D cosmic shear to constrain cosmologies with parameters Omega(M), Omega(B), sigma(8), h , n(s), w(0) and w(a). For a non-evolving dark energy equation of state, and assuming a flat cosmology, lensing combined with Wilkinson Microwave Anisotropy Probe 7 results in h = 0.78 +/- 0.12, Omega(M) = 0.252 +/- 0.079, sigma(8) = 0.88 +/- 0.23 and w = -1.16 +/- 0.38 using only scales k a parts per thousand currency sign 1.5 h Mpc(-1). We also present results of lensing combined with first year Planck results, where we find no tension with the results from this analysis, but we also find no significant improvement over the Planck results alone. We find evidence of a suppression of power compared to Lambda cold dark matter (LCDM) on small scales 1.5 < k a parts per thousand currency sign 5.0 h Mpc(-1) in the lensing data, which is consistent with predictions of the effect of baryonic feedback on the matter power spectrum.
C1 [Kitching, T. D.] Univ Coll London, Mullard Space Sci Lab, Dorking RH5 6NT, Surrey, England.
[Heavens, A. F.; Alsing, J.; Jaffe, A.] Univ London Imperial Coll Sci Technol & Med, Imperial Ctr Inference & Cosmol, London SW7 2AZ, England.
[Erben, T.; Hildebrandt, H.; Schrabback, T.] Univ Bonn, Argelander Inst Astron, D-53121 Bonn, Germany.
[Heymans, C.] Univ Edinburgh, Inst Astron, SUPA, Royal Observ, Edinburgh EH9 3HJ, Midlothian, Scotland.
[Hildebrandt, H.; van Waerbeke, L.; Benjamin, J.] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada.
[Hoekstra, H.; Kuijken, K.; Schrabback, T.; Semboloni, E.; Velander, M.] Leiden Univ, Leiden Observ, NL-2333 CA Leiden, Netherlands.
[Kiessling, A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Mellier, Y.] CNRS, Inst Astrophys Paris, UMR 7095, F-75014 Paris, France.
[Mellier, Y.; Kilbinger, M.] CEA, Irfu, SAp Saclay, Lab AIM, F-91191 Gif Sur Yvette, France.
[Miller, L.; Velander, M.] Univ Oxford, Dept Phys, Oxford OX1 3RH, England.
[Coupon, J.] Univ Geneva, Astron Observ, CH-1290 Versoix, Switzerland.
[Fu, L.] Shanghai Normal Univ, Shanghai Key Lab Astrophys, Shanghai 200234, Peoples R China.
[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.
[Rowe, B. T. P.] UCL, Dept Phys & Astron, London WC1E 6BT, England.
[Schrabback, T.] Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, Stanford, CA 94305 USA.
RP Kitching, TD (reprint author), Univ Coll London, Mullard Space Sci Lab, Holmbury St Mary, Dorking RH5 6NT, Surrey, England.
EM t.kitching@ucl.ac.uk
RI Hudson, Michael/H-3238-2012; Fu, Liping/B-3051-2012;
OI Hudson, Michael/0000-0002-1437-3786; Kiessling,
Alina/0000-0002-2590-1273; Rowe, Barnaby/0000-0002-7042-9174; Kilbinger,
Martin/0000-0001-9513-7138; Hoekstra, Henk/0000-0002-0641-3231
FU Royal Society University
FX We thank Dipak Munshi, Andy Taylor, Fergus Simpson, Stephen Feeney,
Hiranya Peiris, Licia Verde, Raul Jimenez, Jason McEwen and Mark Cropper
for useful discussions. We thank Anthony Lewis and the developers of
CAMB, and the PPF module for making their code public. We thank Eric
Tittley and Mark Holliman for system administration on several machines
used in this work. We made use of CosmoCalc http://www.astro.ucla.
edu/wright/CosmoCalc.html (Wright 2006) during development. We thank
WMAP for providing their MCMC chains available for download
http://lambda.gsfc.nasa.gov, and Eiichiro Komatsu for providing
supplementary data products to the main WMAP data release. We thank ESA
Planck for providing their MCMC chains available for download
http://pla.esac.esa.int/pla/aio/planckProducts.html. TDK acknowledges
support from a Royal Society University Research Fellowship.
NR 81
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Z9 47
U1 0
U2 3
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 AUG 1
PY 2014
VL 442
IS 2
BP 1326
EP 1349
DI 10.1093/mnras/stu934
PG 24
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AL8XM
UT WOS:000339423100032
ER
PT J
AU Goncalves, TS
Basu-Zych, A
Overzier, RA
Perez, L
Martin, DC
AF Goncalves, Thiago S.
Basu-Zych, Antara
Overzier, Roderik A.
Perez, Laura
Martin, D. Christopher
TI Molecular gas properties of UV-bright star-forming galaxies at low
redshift
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE galaxies: formation; galaxies: ISM; galaxies: starburst
ID LYMAN BREAK GALAXY; ULTRAVIOLET-LUMINOUS GALAXIES; MASS-METALLICITY
RELATION; CO-TO-H-2 CONVERSION FACTOR; DIGITAL SKY SURVEY; ULTRA DEEP
FIELD; NEARBY GALAXIES; FORMATION LAW; SUBMILLIMETER GALAXIES; DISK
GALAXIES
AB Lyman break analogues (LBAs) are a population of star-forming galaxies at low redshift (z similar to 0.2) selected in the ultraviolet (UV). These objects present higher star formation rates and lower dust extinction than other galaxies with similar masses and luminosities in the local universe. In this work, we present results from a survey with the Combined Array for Research in Millimeter-wave Astronomy (CARMA) array to detect CO(1-0) emission in LBAs, in order to analyse the properties of the molecular gas in these galaxies. Our results show that LBAs follow the same Schmidt-Kennicutt law as local galaxies. On the other hand, they have higher gas fractions (up to 66 per cent) and faster gas depletion time-scales (below 1 Gyr). These characteristics render these objects more akin to high-redshift star-forming galaxies. We conclude that LBAs are a great nearby laboratory for studying the cold interstellar medium in low-metallicity, UV-bright compact star-forming galaxies.
C1 [Goncalves, Thiago S.] Univ Fed Rio de Janeiro, Observ Valongo, BR-20080090 Rio De Janeiro, RJ, Brazil.
[Basu-Zych, Antara] NASA, Goddard Space Flight Ctr, Lab Xray Astrophys, Greenbelt, MD 20771 USA.
[Overzier, Roderik A.] Observ Nacl, BR-20921400 Rio De Janeiro, RJ, Brazil.
[Perez, Laura] Natl Radio Astron Observ, Socorro, NM 87801 USA.
[Martin, D. Christopher] CALTECH, Pasadena, CA 91125 USA.
RP Goncalves, TS (reprint author), Univ Fed Rio de Janeiro, Observ Valongo, Ladeira Pedro Antonio 43, BR-20080090 Rio De Janeiro, RJ, Brazil.
EM tsg@astro.ufrj.br
FU CAPES (Coordenacao de Aperfeicoamento de Pessoal de Nivel Superior)
FX We thank the anonymous referee for suggestions that helped improve this
paper. We would also like to thank Andrew Baker and Tim Heckman for
useful comments. TSG gratefully acknowledges CAPES (Coordenacao de
Aperfeicoamento de Pessoal de Nivel Superior) for financial support.
Support for CARMA construction was derived from the states of
California, Illinois, and Maryland, the James S. McDonnell Foundation,
the Gordon and Betty Moore Foundation, the Kenneth T. and Eileen L.
Norris Foundation, the University of Chicago, the Associates of the
California Institute of Technology, and the National Science Foundation.
Ongoing CARMA development and operations are supported by the National
Science Foundation under a cooperative agreement, and by the CARMA
partner universities.
NR 81
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U1 0
U2 3
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 AUG 1
PY 2014
VL 442
IS 2
BP 1429
EP 1439
DI 10.1093/mnras/stu852
PG 11
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AL8XM
UT WOS:000339423100039
ER
PT J
AU Huang, H
Cao, YW
Xie, GD
Ren, YX
Yan, Y
Bao, CJ
Ahmed, N
Neifeld, MA
Dolinar, SJ
Willner, AE
AF Huang, Hao
Cao, Yinwen
Xie, Guodong
Ren, Yongxiong
Yan, Yan
Bao, Changjing
Ahmed, Nisar
Neifeld, Mark A.
Dolinar, Samuel J.
Willner, Alan E.
TI Crosstalk mitigation in a free-space orbital angular momentum
multiplexed communication link using 4x4 MIMO equalization
SO OPTICS LETTERS
LA English
DT Article
ID ATMOSPHERIC-TURBULENCE; SINGLE-PHOTON; TRANSMISSION; FIBER;
POLARIZATION; SYSTEMS; LIGHT
AB We demonstrate crosstalk mitigation using 4 x 4 multiple-input-multiple-output (MIMO) equalization on an orbital angular momentum (OAM) multiplexed free-space data link with heterodyne detection. Four multiplexed OAM beams, each carrying a 20 Gbit/s quadrature phase-shift keying signal, propagate through weak turbulence. The turbulence induces inter-channel crosstalk among each beam and degrades the signal performance. Experimental results demonstrate that with the assistance of MIMO processing, the signal quality and the bit-error-rate (BER) performance can be improved. The power penalty can be reduced by >4 dB at a BER of 3.8 x 10(-3). (C) 2014 Optical Society of America
C1 [Huang, Hao; Cao, Yinwen; Xie, Guodong; Ren, Yongxiong; Yan, Yan; Bao, Changjing; Ahmed, Nisar; Willner, Alan E.] Univ So Calif, Dept Elect Engn, Los Angeles, CA 90089 USA.
[Neifeld, Mark A.] Univ Arizona, Dept Elect & Comp Engn, Tucson, AZ 85721 USA.
[Dolinar, Samuel J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Huang, H (reprint author), Univ So Calif, Dept Elect Engn, Los Angeles, CA 90089 USA.
EM haoh@usc.edu
FU DARPA under the InPho (Information in a Photon) program
FX We acknowledge the support of DARPA under the InPho (Information in a
Photon) program.
NR 24
TC 19
Z9 20
U1 0
U2 23
PU OPTICAL SOC AMER
PI WASHINGTON
PA 2010 MASSACHUSETTS AVE NW, WASHINGTON, DC 20036 USA
SN 0146-9592
EI 1539-4794
J9 OPT LETT
JI Opt. Lett.
PD AUG 1
PY 2014
VL 39
IS 15
BP 4360
EP 4363
DI 10.1364/OL.39.004360
PG 4
WC Optics
SC Optics
GA AM5EL
UT WOS:000339878900020
PM 25078177
ER
PT J
AU Ackermann, M
Ajello, M
Albert, A
Baldini, L
Ballet, J
Barbiellini, G
Bastieri, D
Bellazzini, R
Bissaldi, E
Blandford, RD
Bloom, ED
Bottacini, E
Brandt, TJ
Bregeon, J
Bruel, P
Buehler, R
Buson, S
Caliandro, GA
Cameron, RA
Caragiulo, M
Caraveo, PA
Cavazzuti, E
Charles, E
Chekhtman, A
Cheung, CC
Chiang, J
Chiaro, G
Ciprini, S
Claus, R
Cohen-Tanugi, J
Conrad, J
Corbel, S
D'Ammando, F
de Angelis, A
den Hartog, PR
de Palma, F
Dermer, CD
Desiante, R
Digel, SW
Di Venere, L
Silva, EDE
Donato, D
Drell, PS
Drlica-Wagner, A
Favuzzi, C
Ferrara, EC
Focke, WB
Franckowiak, A
Fuhrmann, L
Fukazawa, Y
Fusco, P
Gargano, F
Gasparrini, D
Germani, S
Giglietto, N
Giordano, F
Giroletti, M
Glanzman, T
Godfrey, G
Grenier, IA
Grove, JE
Guiriec, S
Hadasch, D
Harding, AK
Hayashida, M
Hays, E
Hewitt, JW
Hill, AB
Hou, X
Jean, P
Jogler, T
Johannesson, G
Johnson, AS
Johnson, WN
Kerr, M
Knodlseder, J
Kuss, M
Larsson, S
Latronico, L
Lemoine-Goumard, M
Longo, F
Loparco, F
Lott, B
Lovellette, MN
Lubrano, P
Manfreda, A
Martin, P
Massaro, F
Mayer, M
Mazziotta, MN
McEnery, JE
Michelson, PF
Mitthumsiri, W
Mizuno, T
Monzani, ME
Morselli, A
Moskalenko, IV
Murgia, S
Nemmen, R
Nuss, E
Ohsugi, T
Omodei, N
Orienti, M
Orlando, E
Ormes, JF
Paneque, D
Panetta, JH
Perkins, JS
Pesce-Rollins, M
Piron, F
Pivato, G
Porter, TA
Raino, S
Rando, R
Razzano, M
Razzaque, S
Reimer, A
Reimer, O
Reposeur, T
Parkinson, PMS
Schaal, M
Schulz, A
Sgro, C
Siskind, EJ
Spandre, G
Spinelli, P
Stawarz, L
Suson, DJ
Takahashi, H
Tanaka, T
Thayer, JG
Thayer, JB
Thompson, DJ
Tibaldo, L
Tinivella, M
Torres, DF
Tosti, G
Troja, E
Uchiyama, Y
Vianello, G
Winer, BL
Wolff, MT
Wood, DL
Wood, KS
Wood, M
Charbonnel, S
Corbet, RHD
Aquino, ID
Edlin, JP
Mason, E
Schwarz, GJ
Shore, SN
Starrfield, S
Teyssier, F
AF Ackermann, M.
Ajello, M.
Albert, A.
Baldini, L.
Ballet, J.
Barbiellini, G.
Bastieri, D.
Bellazzini, R.
Bissaldi, E.
Blandford, R. D.
Bloom, E. D.
Bottacini, E.
Brandt, T. J.
Bregeon, J.
Bruel, P.
Buehler, R.
Buson, S.
Caliandro, G. A.
Cameron, R. A.
Caragiulo, M.
Caraveo, P. A.
Cavazzuti, E.
Charles, E.
Chekhtman, A.
Cheung, C. C.
Chiang, J.
Chiaro, G.
Ciprini, S.
Claus, R.
Cohen-Tanugi, J.
Conrad, J.
Corbel, S.
D'Ammando, F.
de Angelis, A.
den Hartog, P. R.
de Palma, F.
Dermer, C. D.
Desiante, R.
Digel, S. W.
Di Venere, L.
do Couto e Silva, E.
Donato, D.
Drell, P. S.
Drlica-Wagner, A.
Favuzzi, C.
Ferrara, E. C.
Focke, W. B.
Franckowiak, A.
Fuhrmann, L.
Fukazawa, Y.
Fusco, P.
Gargano, F.
Gasparrini, D.
Germani, S.
Giglietto, N.
Giordano, F.
Giroletti, M.
Glanzman, T.
Godfrey, G.
Grenier, I. A.
Grove, J. E.
Guiriec, S.
Hadasch, D.
Harding, A. K.
Hayashida, M.
Hays, E.
Hewitt, J. W.
Hill, A. B.
Hou, X.
Jean, P.
Jogler, T.
Johannesson, G.
Johnson, A. S.
Johnson, W. N.
Kerr, M.
Knoedlseder, J.
Kuss, M.
Larsson, S.
Latronico, L.
Lemoine-Goumard, M.
Longo, F.
Loparco, F.
Lott, B.
Lovellette, M. N.
Lubrano, P.
Manfreda, A.
Martin, P.
Massaro, F.
Mayer, M.
Mazziotta, M. N.
McEnery, J. E.
Michelson, P. F.
Mitthumsiri, W.
Mizuno, T.
Monzani, M. E.
Morselli, A.
Moskalenko, I. V.
Murgia, S.
Nemmen, R.
Nuss, E.
Ohsugi, T.
Omodei, N.
Orienti, M.
Orlando, E.
Ormes, J. F.
Paneque, D.
Panetta, J. H.
Perkins, J. S.
Pesce-Rollins, M.
Piron, F.
Pivato, G.
Porter, T. A.
Raino, S.
Rando, R.
Razzano, M.
Razzaque, S.
Reimer, A.
Reimer, O.
Reposeur, T.
Parkinson, P. M. Saz
Schaal, M.
Schulz, A.
Sgro, C.
Siskind, E. J.
Spandre, G.
Spinelli, P.
Stawarz, L.
Suson, D. J.
Takahashi, H.
Tanaka, T.
Thayer, J. G.
Thayer, J. B.
Thompson, D. J.
Tibaldo, L.
Tinivella, M.
Torres, D. F.
Tosti, G.
Troja, E.
Uchiyama, Y.
Vianello, G.
Winer, B. L.
Wolff, M. T.
Wood, D. L.
Wood, K. S.
Wood, M.
Charbonnel, S.
Corbet, R. H. D.
Aquino, I. De Gennaro
Edlin, J. P.
Mason, E.
Schwarz, G. J.
Shore, S. N.
Starrfield, S.
Teyssier, F.
CA Fermi-LAT Collaboration
TI Fermi establishes classical novae as a distinct class of gamma-ray
sources
SO SCIENCE
LA English
DT Article
ID V407 CYGNI; EMISSION; ACCELERATION; SUBCLASS; OUTBURST
AB A classical nova results from runaway thermonuclear explosions on the surface of a white dwarf that accretes matter from a low-mass main-sequence stellar companion. In 2012 and 2013, three novae were detected in gamma rays and stood in contrast to the first gamma-ray-detected nova V407 Cygni 2010, which belongs to a rare class of symbiotic binary systems. Despite likely differences in the compositions and masses of their white dwarf progenitors, the three classical novae are similarly characterized as soft-spectrum transient gamma-ray sources detected over 2- to 3-week durations. The gamma-ray detections point to unexpected high-energy particle acceleration processes linked to the mass ejection from thermonuclear explosions in an unanticipated class of Galactic gamma-ray sources.
C1 [Ackermann, M.; Buehler, R.; Mayer, M.; Schulz, A.] Deutsch Elektronen Synchrotron DESY, D-15738 Zeuthen, Germany.
[Ajello, M.] Clemson Univ, Dept Phys & Astron, Kinard Lab Phys, Clemson, SC 29634 USA.
[Albert, A.; Blandford, R. D.; Bloom, E. D.; Bottacini, E.; Caliandro, G. A.; Cameron, R. A.; Charles, E.; Chiang, J.; Claus, R.; den Hartog, P. R.; Digel, S. W.; do Couto e Silva, E.; Drell, P. S.; Focke, W. B.; Franckowiak, A.; Glanzman, T.; Godfrey, G.; Hill, A. B.; Jogler, T.; Johnson, A. S.; Michelson, P. F.; Mitthumsiri, W.; Monzani, M. E.; Moskalenko, I. V.; Omodei, N.; Orlando, E.; Paneque, D.; Panetta, J. H.; Porter, T. A.; Reimer, A.; Reimer, O.; Thayer, J. G.; Thayer, J. B.; Tibaldo, L.; Vianello, G.; Wood, M.] Stanford Univ, WW Hansen Expt Phys Lab, Kavli Inst Particle Astrophys & Cosmol, Dept Phys, Stanford, CA 94305 USA.
[Albert, A.; Blandford, R. D.; Bloom, E. D.; Bottacini, E.; Caliandro, G. A.; Cameron, R. A.; Charles, E.; Chekhtman, A.; Chiang, J.; Claus, R.; den Hartog, P. R.; Digel, S. W.; do Couto e Silva, E.; Drell, P. S.; Focke, W. B.; Franckowiak, A.; Glanzman, T.; Godfrey, G.; Hill, A. B.; Jogler, T.; Johnson, A. S.; Michelson, P. F.; Mitthumsiri, W.; Monzani, M. E.; Moskalenko, I. V.; Omodei, N.; Orlando, E.; Paneque, D.; Panetta, J. H.; Porter, T. A.; Reimer, A.; Reimer, O.; Thayer, J. G.; Thayer, J. B.; Tibaldo, L.; Vianello, G.; Wood, M.] Stanford Univ, SLAC Natl Accelerator Lab, Stanford, CA 94305 USA.
[Baldini, L.; Bellazzini, R.; Kuss, M.; Manfreda, A.; Pesce-Rollins, M.; Razzano, M.; Sgro, C.; Spandre, G.; Tinivella, M.; Shore, S. N.] Ist Nazl Fis Nucl, Sez Pisa, I-56127 Pisa, Italy.
[Ballet, J.; Corbel, S.; Rando, R.] Univ Paris Diderot, CNRS, CEA IRFU, Lab AIM,Serv Astrophys,CEA Saclay, F-91191 Gif Sur Yvette, France.
[Barbiellini, G.; Desiante, R.; Grenier, I. A.; Longo, F.] Ist Nazl Fis Nucl, Sez Trieste, I-34127 Trieste, Italy.
[Barbiellini, G.; Longo, F.] Univ Trieste, Dipartimento Fis, I-34127 Trieste, Italy.
[Bastieri, D.; Buson, S.; Rando, R.] Ist Nazl Fis Nucl, Sez Padova, I-35131 Padua, Italy.
[Bastieri, D.; Buson, S.; Chiaro, G.; Pivato, G.] Univ Padua, Dipartimento Fis & Astron G Galilei, I-35131 Padua, Italy.
[Bissaldi, E.] Ist Nazl Fis Nucl, Sez Trieste, I-34127 Trieste, Italy.
[Bissaldi, E.] Univ Trieste, I-34127 Trieste, Italy.
[Brandt, T. J.; Donato, D.; Ferrara, E. C.; Guiriec, S.; Harding, A. K.; Hays, E.; Hewitt, J. W.; McEnery, J. E.; Nemmen, R.; Perkins, J. S.; Thompson, D. J.; Troja, E.; Corbet, R. H. D.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Bregeon, J.; Cohen-Tanugi, J.; Nuss, E.; Piron, F.] Univ Montpellier 2, CNRS, IN2P3, Lab Univers & Particules Montpellier, Montpellier, France.
[Bruel, P.] Ecole Polytech, CNRS, IN2P3, Lab Leprince Ringuet, F-91128 Palaiseau, France.
[Caliandro, G. A.] CIFS, I-10133 Turin, Italy.
[Caragiulo, M.; de Palma, F.; Favuzzi, C.; Fusco, P.; Gargano, F.; Giglietto, N.; Giordano, F.; Loparco, F.; Mazziotta, M. N.; Raino, S.; Spinelli, P.] Ist Nazl Fis Nucl, Sez Bari, I-70126 Bari, Italy.
[Caraveo, P. A.] INAF Ist Astrofis Spaziale & Fis Cosm, I-20133 Milan, Italy.
[Cavazzuti, E.; Ciprini, S.; Gasparrini, D.] ASI Sci Data Ctr, I-00133 Rome, Italy.
[Chekhtman, A.] George Mason Univ, Coll Sci, Ctr Earth Observing & Space Res, Fairfax, VA 22030 USA.
[Cheung, C. C.; Dermer, C. D.; Grove, J. E.; Johnson, W. N.; Lovellette, M. N.; Wolff, M. T.; Wood, K. S.] Naval Res Lab, Div Space Sci, Washington, DC 20375 USA.
[Ciprini, S.; Gasparrini, D.] Osserv Astron Roma, Ist Nazl Astrofis, I-00040 Monte Porzio Catone, Roma, Italy.
[Conrad, J.; Larsson, S.] Stockholm Univ, AlbaNova, Dept Phys, SE-10691 Stockholm, Sweden.
[Conrad, J.; Larsson, S.] AlbaNova, Oskar Klein Ctr Cosmoparticle Phys, SE-10691 Stockholm, Sweden.
[Conrad, J.] Royal Swedish Acad Sci, SE-10405 Stockholm, Sweden.
[Corbel, S.] Inst Univ France, F-75005 Paris, France.
[D'Ammando, F.; Giroletti, M.; Orienti, M.] INAF Ist Radioastron, I-40129 Bologna, Italy.
[D'Ammando, F.] Univ Bologna, Dipartimento Astron, I-40127 Bologna, Italy.
[de Angelis, A.] Univ Udine, Dipartimento Fis, I-33100 Udine, Italy.
[de Angelis, A.] Ist Nazl Fis Nucl, Sez Trieste, Grp Collegato Udine, I-33100 Udine, Italy.
[Desiante, R.] Univ Udine, I-33100 Udine, Italy.
[Di Venere, L.; Favuzzi, C.; Fusco, P.; Giglietto, N.; Giordano, F.; Loparco, F.; Raino, S.; Spinelli, P.] Univ Bari, Dipartimento Fis M Merlin, I-70126 Bari, Italy.
[Di Venere, L.; Favuzzi, C.; Fusco, P.; Giglietto, N.; Giordano, F.; Loparco, F.; Raino, S.; Spinelli, P.] Politecn Bari, I-70126 Bari, Italy.
[Donato, D.; Hewitt, J. W.; Nemmen, R.; Corbet, R. H. D.] CRESST, Greenbelt, MD 20771 USA.
[Donato, D.; McEnery, J. E.; Troja, E.] Univ Maryland, Dept Phys, College Pk, MD 20742 USA.
[Donato, D.; McEnery, J. E.; Troja, E.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Drlica-Wagner, A.] Fermilab Natl Accelerator Lab, Batavia, IL 60510 USA.
[Fuhrmann, L.] Max Planck Inst Radioastron, D-53121 Bonn, Germany.
[Fukazawa, Y.; Takahashi, H.] Hiroshima Univ, Dept Phys Sci, Hiroshima 7398526, Japan.
[Germani, S.; Lubrano, P.; Tosti, G.] Ist Nazl Fis Nucl, Sez Perugia, I-06123 Perugia, Italy.
[Germani, S.; Lubrano, P.; Tosti, G.] Univ Perugia, Dipartimento Fis, I-06123 Perugia, Italy.
[Hadasch, D.; Reimer, A.; Reimer, O.] Univ Innsbruck, Inst Astro & Teilchenphys, A-6020 Innsbruck, Austria.
[Hadasch, D.; Reimer, A.; Reimer, O.] Univ Innsbruck, Inst Theoret Phys, A-6020 Innsbruck, Austria.
[Hayashida, M.] Univ Tokyo, Inst Cosm Ray Res, Kashiwa, Chiba 2778582, Japan.
[Hewitt, J. W.; Nemmen, R.; Corbet, R. H. D.] Univ Maryland Baltimore Cty, Dept Phys, Baltimore, MD 21250 USA.
[Hewitt, J. W.; Nemmen, R.; Corbet, R. H. D.] Univ Maryland Baltimore Cty, Ctr Space Sci & Technol, Baltimore, MD 21250 USA.
[Hill, A. B.] Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England.
[Hou, X.; Lemoine-Goumard, M.; Lott, B.; Reposeur, T.] Univ Bordeaux 1, CNRS, IN2P3, Ctr Etud Nucl Bordeaux Gradignan, F-33175 Gradignan, France.
[Jean, P.; Knoedlseder, J.] CNRS, IRAP, F-31028 Toulouse 4, France.
[Jean, P.; Knoedlseder, J.; Martin, P.] Univ Toulouse, GAHEC, IRAP, UPS OMP, Toulouse, France.
[Johannesson, G.] Univ Iceland, Inst Sci, IS-107 Reykjavik, Iceland.
[Kerr, M.] Australia Telescope Natl Facil, CSIRO Astron & Space Sci, Epping, NSW 1710, Australia.
[Larsson, S.] Stockholm Univ, Dept Astron, SE-10691 Stockholm, Sweden.
[Latronico, L.] Ist Nazl Fis Nucl, Sez Torino, I-10125 Turin, Italy.
[Massaro, F.] Yale Univ, Dept Phys, Dept Astron, New Haven, CT 06520 USA.
[Massaro, F.] Yale Univ, Yale Ctr Astron & Astrophys, New Haven, CT 06520 USA.
[Mitthumsiri, W.] Mahidol Univ, Fac Sci, Dept Phys, Bangkok 10400, Thailand.
[Mizuno, T.; Ohsugi, T.] Hiroshima Univ, Hiroshima Astrophys Sci Ctr, Hiroshima 7398526, Japan.
[Morselli, A.] Ist Nazl Fis Nucl, Sez Roma Tor Vergata, I-00133 Rome, Italy.
[Murgia, S.] Univ Calif Irvine, Ctr Cosmol, Dept Phys & Astron, Irvine, CA 92697 USA.
[Ormes, J. F.] Univ Denver, Dept Phys & Astron, Denver, CO 80208 USA.
[Paneque, D.] Max Planck Inst Phys & Astrophys, D-80805 Munich, Germany.
[Razzaque, S.] Univ Johannesburg, Dept Phys, ZA-2006 Auckland Pk, South Africa.
[Parkinson, P. M. Saz] Univ Calif Santa Cruz, Dept Phys, Santa Cruz Inst Particle Phys, Santa Cruz, CA 95064 USA.
[Parkinson, P. M. Saz] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA.
[Parkinson, P. M. Saz] Univ Hong Kong, Dept Phys, Hong Kong, Hong Kong, Peoples R China.
[Schaal, M.] Natl Acad Sci, Natl Res Council Res Associate, Washington, DC 20001 USA.
[Siskind, E. J.] NYCB Real Time Comp Inc, Lattingtown, NY 11560 USA.
[Stawarz, L.] Japan Aerosp Explorat Agcy, Inst Space & Astronaut Sci, Chuo Ku, Sagamihara, Kanagawa 2525210, Japan.
[Stawarz, L.] Jagiellonian Univ, Astron Observ, PL-30244 Krakow, Poland.
[Suson, D. J.] Purdue Univ Calumet, Dept Chem & Phys, Hammond, IN 46323 USA.
[Tanaka, T.] Kyoto Univ, Dept Phys, Grad Sch Sci, Kyoto 606, Japan.
[Torres, D. F.] Inst Ciencies Espai IEEE CSIC, Barcelona 08193, Spain.
[Torres, D. F.] ICREA, Barcelona, Spain.
[Winer, B. L.] Ohio State Univ, Dept Phys, Ctr Cosmol & Astroparticle Phys, Columbus, OH 43210 USA.
[Wood, D. L.] Praxis Inc, Alexandria, VA 22303 USA.
[Charbonnel, S.] Durtal Observ, F-49430 Durtal, France.
[Aquino, I. De Gennaro; Shore, S. N.] Univ Pisa, Dipartimento Fis Enrico Fermi, I-56127 Pisa, Italy.
[Aquino, I. De Gennaro] Hamburger Sternwarte, D-21029 Hamburg, Germany.
[Edlin, J. P.] Ammon, Idaho Falls, ID 83401 USA.
[Mason, E.] INAF Osservatorio Astron Trieste, I-34131 Trieste, Italy.
[Schwarz, G. J.] Amer Astron Soc, Washington, DC 20009 USA.
[Starrfield, S.] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85287 USA.
RP Cheung, CC (reprint author), Naval Res Lab, Div Space Sci, Washington, DC 20375 USA.
EM teddy.cheung@nrl.navy.mil; pierre.jean@irap.omp.eu; shore@df.unipi.it
RI Orlando, E/R-5594-2016; Di Venere, Leonardo/C-7619-2017; Torres,
Diego/O-9422-2016; Morselli, Aldo/G-6769-2011; Nemmen,
Rodrigo/O-6841-2014; Reimer, Olaf/A-3117-2013; Johannesson,
Gudlaugur/O-8741-2015; Loparco, Francesco/O-8847-2015; Mazziotta, Mario
/O-8867-2015; Gargano, Fabio/O-8934-2015; giglietto, nicola/I-8951-2012;
Moskalenko, Igor/A-1301-2007; Sgro, Carmelo/K-3395-2016; Bissaldi,
Elisabetta/K-7911-2016; Massaro, Francesco/L-9102-2016
OI Di Venere, Leonardo/0000-0003-0703-824X; mason,
elena/0000-0003-3877-0484; SPINELLI, Paolo/0000-0001-6688-8864; Hill,
Adam/0000-0003-3470-4834; Torres, Diego/0000-0002-1522-9065; Morselli,
Aldo/0000-0002-7704-9553; Reimer, Olaf/0000-0001-6953-1385; Johannesson,
Gudlaugur/0000-0003-1458-7036; Loparco, Francesco/0000-0002-1173-5673;
Mazziotta, Mario /0000-0001-9325-4672; Gargano,
Fabio/0000-0002-5055-6395; giglietto, nicola/0000-0002-9021-2888;
Moskalenko, Igor/0000-0001-6141-458X; Bissaldi,
Elisabetta/0000-0001-9935-8106; Massaro, Francesco/0000-0002-1704-9850
FU Naval Research Laboratory by a Karles' Fellowship; NASA through DPR
program [S-15633-Y]; NASA through Guest Investigator program
[11-FERMI11-0030, 12-FERMI12-0026]; NASA; NSF
FX The Fermi-LAT Collaboration acknowledges support for LAT development,
operation, and data analysis from NASA and the Department of Energy
(United States), CEA/Irfu and IN2P3/CNRS (France), Agenzia Spaziale
Italiana and INFN (Italy), MEXT, KEK, and JAXA (Japan), and the K. A.
Wallenberg Foundation, the Swedish Research Council, and the National
Space Board (Sweden). Science analysis support in the operations phase
from INAF (Italy) and CNES (France) is also gratefully acknowledged. We
acknowledge with thanks the variable star observations from the American
Association of Variable Star Observers International Database
contributed by observers worldwide and used in this research and the
dedicated observers of the Astronomical Ring for Access to Spectroscopy
(ARAS) group for their tireless and selfless efforts. C.C.C. was
supported at the Naval Research Laboratory by a Karles' Fellowship and
by NASA through DPR S-15633-Y and Guest Investigator programs
11-FERMI11-0030 and 12-FERMI12-0026. S. S. was supported by NASA and NSF
grants to Arizona State University. The Fermi-LAT data reported in this
paper are available from http://fermi.gsfc.nasa.gov/ssc/data/access.
NR 28
TC 35
Z9 36
U1 1
U2 32
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 AUG 1
PY 2014
VL 345
IS 6196
BP 554
EP 558
DI 10.1126/science.1253947
PG 5
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA AM2AU
UT WOS:000339651300043
ER
PT J
AU Mellon, MT
Mckay, CP
Heldmann, JL
AF Mellon, Michael T.
Mckay, Christopher P.
Heldmann, Jennifer L.
TI Polygonal ground in the McMurdo Dry Valleys of Antarctica and its
relationship to ice-table depth and the recent Antarctic climate history
SO ANTARCTIC SCIENCE
LA English
DT Article
DE Beacon Valley; ground ice; permafrost; polygon
ID MIOCENE GLACIER ICE; BEACON VALLEY; PERMAFROST DISTRIBUTION; REGION;
MARS; SUBLIMATION; STABILITY; ORIGIN; CREEP; SNOW
AB The occurrence of dry permafrost overlying ice-rich permafrost is unique to the Antarctic Dry Valleys on Earth and to the high latitudes of Mars. The stability and distribution of this ice are poorly understood and fundamental to understanding the Antarctic climate as far back as a few million years. Polygonal patterned ground is nearly ubiquitous in these regions and is integrally linked to the history of the icy permafrost and climate. We examined the morphology of polygonal ground in Beacon Valley and the Beacon Heights region of the Antarctic Dry Valleys, and show that polygon size is correlated with ice-table depth (the boundary between dry and ice-rich permafrost). A numerical model of seasonal stress in permafrost shows that the ice-table depth is a dominant factor. Remote sensing and field observations of polygon size are therefore important tools for investigating subsurface ice. Polygons are long-lived landforms and observed characteristics indicate no major fluctuations in the ice-table depth during their development. We conclude that the Beacon Valley and Beacon Heights polygons have developed for at least 10(4) years to achieve their present mature-stage morphology and that the ice-table depth has been stable for a similar length of time.
C1 [Mellon, Michael T.] SW Res Inst, Dept Space Studies, Boulder, CO 80302 USA.
[Mckay, Christopher P.; Heldmann, Jennifer L.] NASA, Ames Res Ctr, Div Space Sci, Moffett Field, CA 94035 USA.
RP Mellon, MT (reprint author), SW Res Inst, Dept Space Studies, 1050 Walnut St, Boulder, CO 80302 USA.
EM mellon@boulder.swri.edu
RI Mellon, Michael/C-3456-2016
FU NASA Planetary Geology and Geophysics programme [NNX08AE33G]; NASA ASTEP
programme; NSF Office of Polar Programs
FX This work was supported in part by the NASA Planetary Geology and
Geophysics programme through grant NNX08AE33G. We also acknowledge
support from the NASA ASTEP programme. Field work in the Antarctic Dry
Valleys was supported by the NSF Office of Polar Programs. We thank
Jaakko Putkonen and an anonymous reviewer for their constructive and
thorough comments.
NR 44
TC 4
Z9 4
U1 1
U2 13
PU CAMBRIDGE UNIV PRESS
PI NEW YORK
PA 32 AVENUE OF THE AMERICAS, NEW YORK, NY 10013-2473 USA
SN 0954-1020
EI 1365-2079
J9 ANTARCT SCI
JI Antarct. Sci.
PD AUG
PY 2014
VL 26
IS 4
BP 413
EP 426
DI 10.1017/S0954102013000710
PG 14
WC Environmental Sciences; Geography, Physical; Geosciences,
Multidisciplinary
SC Environmental Sciences & Ecology; Physical Geography; Geology
GA AL8GX
UT WOS:000339377300012
ER
PT J
AU Johnston, SL
Blue, RS
Jennings, RT
Tarver, WJ
Gray, GW
AF Johnston, Smith L.
Blue, Rebecca S.
Jennings, Richard T.
Tarver, William J.
Gray, Gary W.
TI Astronaut Medical Selection During the Shuttle Era: 1981-2011
SO AVIATION SPACE AND ENVIRONMENTAL MEDICINE
LA English
DT Article
DE spaceflight; medical standards; crewmembers; medical screening
AB Introduction: U.S. astronauts undergo extensive job-related screening and medical examinations prior to selection in order to identify candidates optimally suited for careers in spaceflight. Screening medical standards evolved over many years and after extensive spaceflight experience. These standards assess health-related risks for each astronaut candidate, minimizing the potential for medical impact on future mission success. This document discusses the evolution of the Shuttleera medical selection standards and the most common reasons for medical disqualification of applicants. Methods: Data for astronaut candidate finalists were compiled from medical records and NASA archives from the period of 1978 to 2004 and were retrospectively reviewed for medically disqualifying conditions. Results: During Shuttle selection cycles, a total of 372 applicants were disqualified due to 425 medical concerns. The most common disqualifying conditions included visual, cardiovascular, psychiatric, and behavioral disorders. During this time period, three major expert panel reviews resulted in refinements and alterations to selection standards for future cycles. Discussion: Shuttle-era screening, testing, and specialist evaluations evolved through periodic expert reviews, evidence-based medicine, and astronaut medical care experience. The Shuttle medical program contributed to the development and implementation of NASA and international standards, longitudinal data collection, improved medical care, and occupational surveillance models. The lessons learned from the Shuttle program serve as the basis for medical selection for the ISS, exploration-class missions, and for those expected to participate in commercial spaceflight.
C1 [Johnston, Smith L.; Blue, Rebecca S.; Jennings, Richard T.; Tarver, William J.; Gray, Gary W.] NASA, Houston, TX USA.
RP Blue, RS (reprint author), Univ Texas Med Branch, Dept Prevent Med & Community Hlth, 301 Univ Blvd, Galveston, TX 77555 USA.
EM rsblue@utmb.edu
NR 11
TC 0
Z9 0
U1 2
U2 3
PU AEROSPACE MEDICAL ASSOC
PI ALEXANDRIA
PA 320 S HENRY ST, ALEXANDRIA, VA 22314-3579 USA
SN 0095-6562
EI 1943-4448
J9 AVIAT SPACE ENVIR MD
JI Aviat. Space Environ. Med.
PD AUG
PY 2014
VL 85
IS 8
BP 823
EP 827
DI 10.3357/ASEM.3968.2014
PG 5
WC Public, Environmental & Occupational Health; Medicine, General &
Internal; Sport Sciences
SC Public, Environmental & Occupational Health; General & Internal
Medicine; Sport Sciences
GA AL9IU
UT WOS:000339455600006
PM 25199124
ER
PT J
AU Anderson, JL
Mertens, CJ
Grajewski, B
Luo, LA
Tseng, CY
Cassinelli, RT
AF Anderson, Jeri L.
Mertens, Christopher J.
Grajewski, Barbara
Luo, Lian
Tseng, Chih-Yu
Cassinelli, Rick T., II
TI Flight Attendant Radiation Dose from Solar Particle Events
SO AVIATION SPACE AND ENVIRONMENTAL MEDICINE
LA English
DT Article
DE absorbed dose; effective dose; conceptus; reproductive health
ID MODEL DEVELOPMENT; EXPOSURE; VALIDATION; ALTITUDES; AIRCREW
AB Introduction: Research has suggested that work as a flight attendant may be related to increased risk for reproductive health effects. Air cabin exposures that may influence reproductive health include radiation dose from galactic cosmic radiation and solar particle events. This paper describes the assessment of radiation dose accrued during solar particle events as part of a reproductive health study of flight attendants. Methods: Solar storm data were obtained from the National Oceanic and Atmospheric Administration Space Weather Prediction Center list of solar proton events affecting the Earth environment to ascertain storms relevant to the two study periods (1992-1996 and 1999-2001). Radiation dose from exposure to solar energetic particles was estimated using the NAIRAS model in conjunction with galactic cosmic radiation dose calculated using the CARI-6P computer program. Results: Seven solar particle events were determined to have potential for significant radiation exposure, two in the first study period and five in the second study period, and over-lapped with 24,807 flight segments. Absorbed (and effective) flight segment doses averaged 6.5 mu Gy (18 mu Sv) and 3.1 mu Gy (8.3 mu Sv) for the first and second study periods, respectively. Maximum doses were as high as 440 mu Gy (1.2 mSv) and 20 flight segments had doses greater than 190 mu Gy (0.5 mSv). Discussion: During solar particle events, a pregnant flight attendant could potentially exceed the equivalent dose limit to the conceptus of 0.5 mSv in a month recommended by the National Council on Radiation Protection and Measurements.
C1 [Anderson, Jeri L.] NIOSH, Cincinnati, OH 45226 USA.
NASA, Langley Res Ctr, Hampton, VA 23665 USA.
RP Anderson, JL (reprint author), NIOSH, 4676 Columbia Pkwy,MS R-14, Cincinnati, OH 45226 USA.
EM JLAnderson@cdc.gov
NR 22
TC 2
Z9 2
U1 2
U2 8
PU AEROSPACE MEDICAL ASSOC
PI ALEXANDRIA
PA 320 S HENRY ST, ALEXANDRIA, VA 22314-3579 USA
SN 0095-6562
EI 1943-4448
J9 AVIAT SPACE ENVIR MD
JI Aviat. Space Environ. Med.
PD AUG
PY 2014
VL 85
IS 8
BP 828
EP 832
DI 10.3357/ASEM.3989.2014
PG 5
WC Public, Environmental & Occupational Health; Medicine, General &
Internal; Sport Sciences
SC Public, Environmental & Occupational Health; General & Internal
Medicine; Sport Sciences
GA AL9IU
UT WOS:000339455600007
PM 25199125
ER
PT J
AU Watson, JT
Bigelow, KA
AF Watson, Jordan T.
Bigelow, Keith A.
TI Trade-offs among Catch, Bycatch, and Landed Value in the American Samoa
Longline Fishery
SO CONSERVATION BIOLOGY
LA English
DT Article
DE Albacore; longline; nontarget species; observer data; sea turtles;
sharks; trade-offs
ID EASTERN PACIFIC-OCEAN; HORIZONTAL MOVEMENTS; DEPTH DISTRIBUTION; PELAGIC
FISHES; BY-CATCH; TUNA; CLOSURES; BEHAVIOR; TIME; CONSERVATION
AB The interspecific preferences of fishes for different depths and habitats suggest fishers could avoid unwanted catches of some species while still effectively targeting other species. In pelagic longline fisheries, albacore (Thunnus alalunga) are often caught in relatively cooler, deeper water (>100 m) than many species of conservation concern (e. g., sea turtles, billfishes, and some sharks) that are caught in shallower water (<100 m). From 2007 to 2011, we examined the depth distributions of hooks for 1154 longline sets (3,406,946 hooks) and recorded captures by hook position on 2642 sets (7,829,498 hooks) in the American Samoa longline fishery. Twenty-three percent of hooks had a settled depth <100 m. Individuals captured in the 3 shallowest hook positions accounted for 18.3% of all bycatch. We analyzed hypothetical impacts for 25 of the most abundant species caught in the fishery by eliminating the 3 shallowest hook positions under scenarios with and without redistribution of these hooks to deeper depths. Distributions varied by species: 45.5% (n = 10) of green sea turtle (Chelonia mydas), 59.5% (n = 626) of shortbill spearfish (Tetrapturus angustirostris), 37.3% (n = 435) of silky shark (Carcharhinus falciformis), and 42.6% (n = 150) of oceanic whitetip shark (C. longimanus) were caught on the 3 shallowest hooks. Eleven percent (n = 20,435) of all tuna and 8.5% (n = 10,374) of albacore were caught on the 3 shallowest hooks. Hook elimination reduced landed value by 1.6-9.2%, and redistribution of hooks increased average annual landed value relative to the status quo by 5-11.7%. Based on these scenarios, redistribution of hooks to deeper depths may provide an economically feasible modification to longline gear that could substantially reduce bycatch for a suite of vulnerable species. Our results suggest that this method may be applicable to deep-set pelagic longline fisheries worldwide.
C1 [Watson, Jordan T.] Univ Hawaii, Joint Inst Marine & Atmospher Res, Honolulu, HI 96822 USA.
[Watson, Jordan T.] Univ Alaska Fairbanks, Sch Fisheries & Ocean Sci, Juneau, AK 99801 USA.
[Bigelow, Keith A.] Natl Marine Fisheries Serv, Pacific Isl Fisheries Sci Ctr, Honolulu, HI 96822 USA.
RP Watson, JT (reprint author), Univ Hawaii, Joint Inst Marine & Atmospher Res, 1000 Pope Rd, Honolulu, HI 96822 USA.
EM jordan.watson@noaa.gov
FU Fisheries Disaster Relief Program; Joint Institute for Marine and
Atmospheric Research [NA09OAR4320075]; National Oceanic and Atmospheric
Administration (NOAA) [NA09OAR4320075]
FX We thank captains and crews of American Samoa based longline vessels and
observers for TDR deployments. We thank S. Kostelnik and R. Kupfer for
TDR data management, E. Fletcher for programming support, and E. Forney
and J. Willson for data access. C. Boggs, D. Curran, P. Dalzell, M. Pan,
Y. Swimmer, and 2 anonymous reviewers provided valuable input. This
project was partially funded by the Fisheries Disaster Relief Program
and by Cooperative Agreement NA09OAR4320075 between the Joint Institute
for Marine and Atmospheric Research and the National Oceanic and
Atmospheric Administration (NOAA). The views expressed herein are those
of the authors and do not necessarily reflect the views of NOAA or any
of its subdivisions.
NR 48
TC 7
Z9 7
U1 2
U2 27
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 AUG
PY 2014
VL 28
IS 4
BP 1012
EP 1022
DI 10.1111/cobi.12268
PG 11
WC Biodiversity Conservation; Ecology; Environmental Sciences
SC Biodiversity & Conservation; Environmental Sciences & Ecology
GA AL9ZB
UT WOS:000339501100013
PM 24628499
ER
PT J
AU Desai, SD
Bertiger, W
Haines, BJ
AF Desai, Shailen D.
Bertiger, Willy
Haines, Bruce J.
TI Self-consistent treatment of tidal variations in the geocenter for
precise orbit determination
SO JOURNAL OF GEODESY
LA English
DT Article
DE Reference frame; Geocenter; Ocean tides; Precise orbit determination;
GPS
ID MEAN SEA-LEVEL; GLOBAL POSITIONING SYSTEM; OCEAN TIDES; ALTIMETER
MISSIONS; GEOSAT ALTIMETRY; TIME-SERIES; TOPEX/POSEIDON; SATELLITE;
JASON-1; GPS
AB We show that the current levels of accuracy being achieved for the precise orbit determination (POD) of low-Earth orbiters demonstrate the need for the self-consistent treatment of tidal variations in the geocenter. Our study uses as an example the POD of the OSTM/Jason-2 satellite altimeter mission based upon Global Positioning System (GPS) tracking data. Current GPS-based POD solutions are demonstrating root-mean-square (RMS) radial orbit accuracy and precision of cm and 1 mm, respectively. Meanwhile, we show that the RMS of three-dimensional tidal geocenter variations is mm, but can be as large as 15 mm, with the largest component along the Earth's spin axis. Our results demonstrate that GPS-based POD of Earth orbiters is best performed using GPS satellite orbit positions that are defined in a reference frame whose origin is at the center of mass of the entire Earth system, including the ocean tides. Errors in the GPS-based POD solutions for OSTM/Jason-2 of mm (3D RMS) and mm (radial RMS) are introduced when tidal geocenter variations are not treated consistently. Nevertheless, inconsistent treatment is measurable in the OSTM/Jason-2 POD solutions and manifests through degraded post-fit tracking data residuals, orbit precision, and relative orbit accuracy. For the latter metric, sea surface height crossover variance is higher by when tidal geocenter variations are treated inconsistently.
C1 [Desai, Shailen D.; Bertiger, Willy; Haines, Bruce J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Desai, SD (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr,M-S 238-600, Pasadena, CA 91109 USA.
EM shailen.desai@jpl.nasa.gov
NR 48
TC 3
Z9 3
U1 2
U2 9
PU SPRINGER
PI NEW YORK
PA 233 SPRING ST, NEW YORK, NY 10013 USA
SN 0949-7714
EI 1432-1394
J9 J GEODESY
JI J. Geodesy
PD AUG
PY 2014
VL 88
IS 8
BP 735
EP 747
DI 10.1007/s00190-014-0718-8
PG 13
WC Geochemistry & Geophysics; Remote Sensing
SC Geochemistry & Geophysics; Remote Sensing
GA AL8WV
UT WOS:000339421400002
ER
PT J
AU Kolli, KK
Effat, MA
Peelukhana, SV
Succop, P
Back, LH
Leesar, MA
Helmy, TA
Imran, A
Banerjee, RK
AF Kolli, Kranthi K.
Effat, M. A.
Peelukhana, Srikara V.
Succop, Paul
Back, Lloyd H.
Leesar, M. A.
Helmy, T. A.
Imran, Arif
Banerjee, R. K.
TI Hyperemia-Free Delineation of Epicardial and Microvascular Impairments
Using a Basal Index
SO ANNALS OF BIOMEDICAL ENGINEERING
LA English
DT Article
DE Coronary disease; FFR; CFR; CDP; Catheterization; Hyperemia-free index
ID FRACTIONAL FLOW RESERVE; PRESSURE-DROP COEFFICIENT; CORONARY LESION
SEVERITY; HEMODYNAMIC END-POINTS; PORCINE MODEL;
CARDIAC-CATHETERIZATION; INTRAVENOUS ADENOSINE; HEART-RATE; STENOSIS;
INTRACORONARY
AB The assessment of functional coronary lesion severity using intracoronary hemodynamic parameters like the pressure-derived fractional flow reserve and the flow-derived coronary flow reserve are known to rely critically on the establishment of maximal hyperemia. We evaluated a hyperemia-free index, basal pressure drop coefficient (bCDP), that combines pressure and velocity for simultaneous assessment of the status of both epicardial and microvascular circulations. In 23 pigs, simultaneous measurements of distal coronary arterial pressure and flow were performed using a dual-sensor tipped guidewire in the settings of both normal and abnormal microcirculation with the presence of epicardial lesions of area stenosis (AS) < 50% and AS > 50%. The bCDP, a parameter based on fundamental fluid dynamics principles, was calculated as the transtenotic pressure-drop divided by the dynamic pressure in the distal vessel, measured under baseline (without hyperemia) conditions. The group mean values of bCDP for normal (84 +/- A 18) and abnormal (124.5 +/- A 15.6) microcirculation were significantly different. Similarly, the mean values of bCDP from AS < 50% (72.5 +/- A 16.1) and AS > 50% (136 +/- A 17.2) were also significantly different (p < 0.05). The bCDP could significantly distinguish between lesions of AS < 50% to AS > 50% under normal microcirculation (52.1 vs. 85.8; p < 0.05) and abnormal microcirculation (84.9 vs. 172; p < 0.05). Further, the bCDP correlated linearly and significantly with the hyperemic parameters FFR (r = 0.42, p < 0.05) and CDP (r = 0.50, p < 0.05). The bCDP is a promising clinical diagnostic parameter that can independently assess the severity of epicardial stenosis and microvascular impairment. We believe that it has an immediate appeal for detection of coronary artery disease if validated clinically.
C1 [Kolli, Kranthi K.; Peelukhana, Srikara V.; Banerjee, R. K.] Univ Cincinnati, Dept Mech & Mat Engn, Cincinnati, OH 45221 USA.
[Effat, M. A.; Helmy, T. A.; Imran, Arif] Univ Cincinnati, Div Cardiovasc Dis, Cincinnati, OH USA.
[Kolli, Kranthi K.; Effat, M. A.; Peelukhana, Srikara V.; Helmy, T. A.; Imran, Arif; Banerjee, R. K.] Vet Affairs Med Ctr, Cincinnati, OH 45267 USA.
[Succop, Paul] Univ Cincinnati, Dept Environm Hlth, Cincinnati, OH USA.
[Back, Lloyd H.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Leesar, M. A.] Univ Alabama Birmingham, Div Cardiovasc Dis, Birmingham, AL 35294 USA.
RP Banerjee, RK (reprint author), Univ Cincinnati, Dept Mech & Mat Engn, 598 Rhodes Hall,POB 210072, Cincinnati, OH 45221 USA.
EM rupak.banerjee@uc.edu
FU Great Rivers Affiliate; National-Scientific Development Grant of
American Heart Association [0755236B, 0335270N]; Department of Veteran
Affairs Merit Review Grant [I01CX000342]
FX The authors are grateful to Dr. Mahesh Krishnamoorthy, Dr. Subhashish
Das Gupta, Marwan Al-Rjoub and Bhaskar Konala of Transport in
Engineering and Medicine Laboratory at University of Cincinnati for
their assistance during the experiments. This study is supported by
Grant-In-Aid of Great Rivers Affiliate, National-Scientific Development
Grant of American Heart Association (Grant reference #s: 0755236B and
0335270N) and a Department of Veteran Affairs Merit Review Grant
(I01CX000342).
NR 36
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U1 0
U2 1
PU SPRINGER
PI NEW YORK
PA 233 SPRING ST, NEW YORK, NY 10013 USA
SN 0090-6964
EI 1573-9686
J9 ANN BIOMED ENG
JI Ann. Biomed. Eng.
PD AUG
PY 2014
VL 42
IS 8
BP 1681
EP 1690
DI 10.1007/s10439-014-1020-x
PG 10
WC Engineering, Biomedical
SC Engineering
GA AL8OP
UT WOS:000339399000009
PM 24806315
ER
PT J
AU Flagey, N
Noriega-Crespo, A
Petric, A
Geballe, TR
AF Flagey, N.
Noriega-Crespo, A.
Petric, A.
Geballe, T. R.
TI PALOMAR/TRIPLESPEC OBSERVATIONS OF SPITZER/MIPSGAL 24 mu m CIRCUMSTELLAR
SHELLS: UNVEILING THE NATURES OF THEIR CENTRAL SOURCES
SO ASTRONOMICAL JOURNAL
LA English
DT Article
DE circumstellar matter; stars: early-type; stars: emission-line, Be;
stars: late-type; stars: variables: S Doradus; stars: Wolf-Rayet
ID WOLF-RAYET STARS; LUMINOUS BLUE VARIABLES; INNER GALACTIC PLANE;
INFRARED CLASSIFICATION SPECTROSCOPY; H-ALPHA SURVEY; MASSIVE STARS;
SPECTRAL-ANALYSES; COMPACT BUBBLES; RED SUPERGIANTS; BAND SPECTRA
AB We present near-IR spectroscopic observations of the central sources in 17 circumstellar shells from a sample of more than 400 "bubbles" discovered in the Spitzer/MIPSGAL 24 mu m survey of the Galactic plane and in the Cygnus-X region. To identify the natures of these shells, we have obtained J, H, and K band spectra with a resolution of similar to 2600 of the stars at their centers. We observed 14 MIPSGAL bubbles (MBs), WR149, and 2 objects in the Cygnus-X region (WR138a and BD+43 3710), our sample being about 2.5 mag fainter in the K band than previous studies of the central sources of MBs. We use spectroscopic diagnostics and spectral libraries of late- and early-type stars to constrain the natures of our targets. We find five late-type giants. The equivalent widths of their CO 2.29 mu m features allow us to determine the spectral types of the stars and hence derive the extinction along the line of sight, distance, and physical size of the shells. We also find 12 early-type stars: in 9 MBs and the 3 comparison objects. We find that the subtype inferred from the near-IR for WR138a (WN9h) and WR149 (WN5h) agrees with that derived from optical observations. A careful analysis of the literature and the environment of BD+43 3710 allows us to rule out the carbon star interpretation previously suggested. Our near-IR spectrum suggests that it is a B5 supergiant. At the centers of the nine MBs, we find a WC5-6 star possibly of low mass, a candidate O5-6 V star, a B0 supergiant, a B/A-type giant, and five luminous blue variable (LBV) candidates. We also report the detections of emission lines arising from at least two shells with typical extents (similar to 10 ''), in agreement with those in the mid-IR. We summarize the findings on the natures of the MBs since their discovery, with 30% of them now known. Most MBs with central sources detected in the near- to mid-IR have been identified and are red and blue giants, supergiants, or stars evolving toward these phases, including, in particular, a handful of newly discovered Wolf-Rayet stars and a significant number of LBV candidates.
C1 [Flagey, N.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Flagey, N.] Inst Astron, Hilo, HI 96720 USA.
[Noriega-Crespo, A.] CALTECH, Ctr Infrared Proc & Anal, Pasadena, CA 91125 USA.
[Noriega-Crespo, A.] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
[Petric, A.] CALTECH, Pasadena, CA 91125 USA.
[Petric, A.; Geballe, T. R.] Gemini North Observ, Hilo, HI 96720 USA.
RP Flagey, N (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM nflagey@jpl.nasa.gov
FU Gemini Observatory
FX The Hale Telescope at Palomar Observatory is operated as part of a
collaborative agreement between the California Institute of Technology
and its divisions, Caltech Optical Observatories and the Jet Propulsion
Laboratory (operated for NASA), and Cornell University. This research
has made use of the SIMBAD database, operated at CDS, Strasbourg,
France, and of the NASA/IPAC Infrared Science Archive, which is operated
by the Jet Propulsion Laboratory, California Institute of Technology,
under contract with the National Aeronautics and Space Administration.
N.F. thanks Francois Ochsenbein for providing the plate scale of the BD
charts, Paul Crowther for his help with some identifications, and the
referee, Dr. Vasilii V. Gvaramadze, for valuable comments that clarified
and improved this paper. T.R.G.s research is supported by the Gemini
Observatory, which is operated by the Association of Universities for
Research in Astronomy, Inc., on behalf of the international Gemini
partnership of Argentina, Australia, Brazil, Canada, Chile, and the
United States of America.
NR 71
TC 10
Z9 10
U1 0
U2 3
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-6256
EI 1538-3881
J9 ASTRON J
JI Astron. J.
PD AUG
PY 2014
VL 148
IS 2
AR 34
DI 10.1088/0004-6256/148/2/34
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AL7OQ
UT WOS:000339324400010
ER
PT J
AU Archer, A
Barnacka, A
Beilicke, M
Benbow, W
Berger, K
Bird, R
Biteau, J
Buckley, JH
Bugaev, V
Byrum, K
Cardenzana, JV
Cerruti, M
Chen, W
Chen, X
Ciupik, L
Connolly, MP
Cui, W
Dickinson, HJ
Dumm, J
Eisch, JD
Falcone, A
Federici, S
Feng, Q
Finley, JP
Fleischhack, H
Fortson, L
Furniss, A
Galante, N
Griffin, S
Griffiths, ST
Grube, J
Gyuk, G
Hakansson, N
Hanna, D
Holder, J
Hughes, G
Johnson, CA
Kaaret, P
Kar, P
Kertzman, M
Khassen, Y
Kieda, D
Krawczynski, H
Kumar, S
Lang, MJ
Maier, G
McArthur, S
McCann, A
Meagher, K
Moriarty, P
Mukherjee, R
Nieto, D
de Bhroithe, AO
Ong, RA
Otte, AN
Park, N
Perkins, JS
Pohl, M
Popkow, A
Prokoph, H
Pueschel, E
Quinn, J
Ragan, K
Rajotte, J
Reyes, LC
Reynolds, PT
Richards, GT
Roache, E
Sembroski, GH
Shahinyan, K
Smith, AW
Staszak, D
Telezhinsky, I
Tucci, JV
Tyler, J
Varlotta, A
Vincent, S
Wakely, SP
Weinstein, A
Welsing, R
Wilhelm, A
Williams, DA
Zajczyk, A
Zitzer, B
AF Archer, A.
Barnacka, A.
Beilicke, M.
Benbow, W.
Berger, K.
Bird, R.
Biteau, J.
Buckley, J. H.
Bugaev, V.
Byrum, K.
Cardenzana, J. V.
Cerruti, M.
Chen, W.
Chen, X.
Ciupik, L.
Connolly, M. P.
Cui, W.
Dickinson, H. J.
Dumm, J.
Eisch, J. D.
Falcone, A.
Federici, S.
Feng, Q.
Finley, J. P.
Fleischhack, H.
Fortson, L.
Furniss, A.
Galante, N.
Griffin, S.
Griffiths, S. T.
Grube, J.
Gyuk, G.
Hakansson, N.
Hanna, D.
Holder, J.
Hughes, G.
Johnson, C. A.
Kaaret, P.
Kar, P.
Kertzman, M.
Khassen, Y.
Kieda, D.
Krawczynski, H.
Kumar, S.
Lang, M. J.
Maier, G.
McArthur, S.
McCann, A.
Meagher, K.
Moriarty, P.
Mukherjee, R.
Nieto, D.
de Bhroithe, A. O'Faolain
Ong, R. A.
Otte, A. N.
Park, N.
Perkins, J. S.
Pohl, M.
Popkow, A.
Prokoph, H.
Pueschel, E.
Quinn, J.
Ragan, K.
Rajotte, J.
Reyes, L. C.
Reynolds, P. T.
Richards, G. T.
Roache, E.
Sembroski, G. H.
Shahinyan, K.
Smith, A. W.
Staszak, D.
Telezhinsky, I.
Tucci, J. V.
Tyler, J.
Varlotta, A.
Vincent, S.
Wakely, S. P.
Weinstein, A.
Welsing, R.
Wilhelm, A.
Williams, D. A.
Zajczyk, A.
Zitzer, B.
TI VERY-HIGH ENERGY OBSERVATIONS OF THE GALACTIC CENTER REGION BY VERITAS
IN 2010-2012
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE astroparticle physics; black hole physics; Galaxy: center; gamma rays:
galaxies; methods: data analysis; radiation mechanisms: non-thermal
ID SGR-A-ASTERISK; GAMMA-RAY SOURCE; MOLECULAR CLOUDS; MAGIC TELESCOPE;
SOURCE CATALOG; DARK-MATTER; CRAB-NEBULA; EMISSION; VARIABILITY;
DISCOVERY
AB The Galactic center is an interesting region for high-energy (0.1-100 GeV) and very-high-energy (E > 100 GeV) gamma-ray observations. Potential sources of GeV/TeV gamma-ray emission have been suggested, e.g., the accretion of matter onto the supermassive black hole, cosmic rays from a nearby supernova remnant (e.g., Sgr A East), particle acceleration in a plerion, or the annihilation of dark matter particles. The Galactic center has been detected by EGRET and by Fermi/LAT in the MeV/GeV energy band. At TeV energies, the Galactic center was detected with moderate significance by the CANGAROO and Whipple 10 m telescopes and with high significance by H.E.S.S., MAGIC, and VERITAS. We present the results from three years of VERITAS observations conducted at large zenith angles resulting in a detection of the Galactic center on the level of 18 standard deviations at energies above similar to 2.5 TeV. The energy spectrum is derived and is found to be compatible with hadronic, leptonic, and hybrid emission models discussed in the literature. Future, more detailed measurements of the high-energy cutoff and better constraints on the high-energy flux variability will help to refine and/or disentangle the individual models.
C1 [Archer, A.; Beilicke, M.; Buckley, J. H.; Bugaev, V.; Chen, W.; Krawczynski, H.; Zajczyk, A.] Washington Univ, Dept Phys, St Louis, MO 63130 USA.
[Barnacka, A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Benbow, W.; Cerruti, M.; Galante, N.; Roache, E.] Harvard Smithsonian Ctr Astrophys, Fred Lawrence Whipple Observ, Amado, AZ 85645 USA.
[Berger, K.; Holder, J.; Kumar, S.] Univ Delaware, Dept Phys & Astron, Newark, DE 19716 USA.
[Berger, K.; Holder, J.; Kumar, S.] Univ Delaware, Bartol Res Inst, Newark, DE 19716 USA.
[Bird, R.; Khassen, Y.; Pueschel, E.; Quinn, J.] Univ Coll Dublin, Sch Phys, Dublin, Ireland.
[Biteau, J.; Furniss, A.; Johnson, C. A.; Williams, D. A.] Univ Calif Santa Cruz, Santa Cruz Inst Particle Phys, Santa Cruz, CA 95064 USA.
[Biteau, J.; Furniss, A.; Johnson, C. A.; Williams, D. A.] Univ Calif Santa Cruz, Dept Phys, Santa Cruz, CA 95064 USA.
[Byrum, K.; Zitzer, B.] Argonne Natl Lab, Argonne, IL 60439 USA.
[Cardenzana, J. V.; Dickinson, H. J.; Eisch, J. D.; Weinstein, A.] Iowa State Univ, Dept Phys & Astron, Ames, IA 50011 USA.
[Chen, X.; Federici, S.; Hakansson, N.; Pohl, M.; Telezhinsky, I.; Wilhelm, A.] Univ Potsdam, Inst Phys & Astron, D-14476 Potsdam, Germany.
[Chen, X.; Federici, S.; Fleischhack, H.; Hughes, G.; Maier, G.; de Bhroithe, A. O'Faolain; Pohl, M.; Prokoph, H.; Telezhinsky, I.; Vincent, S.; Welsing, R.; Wilhelm, A.] DESY, D-15738 Zeuthen, Germany.
[Ciupik, L.; Grube, J.; Gyuk, G.] Adler Planetarium & Astron Museum, Dept Astron, Chicago, IL 60605 USA.
[Connolly, M. P.; Lang, M. J.; Moriarty, P.] Natl Univ Ireland Galway, Sch Phys, Galway, Ireland.
[Cui, W.; Feng, Q.; Finley, J. P.; Sembroski, G. H.; Tucci, J. V.; Varlotta, A.] Purdue Univ, Dept Phys & Astron, W Lafayette, IN 47907 USA.
[Dumm, J.; Fortson, L.; Shahinyan, K.] Univ Minnesota, Sch Phys & Astron, Minneapolis, MN 55455 USA.
[Falcone, A.] Penn State Univ, Dept Astron & Astrophys, Davey Lab 525, University Pk, PA 16802 USA.
[Griffin, S.; Hanna, D.; Ragan, K.; Rajotte, J.; Staszak, D.; Tyler, J.] McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada.
[Griffiths, S. T.; Kaaret, P.] Univ Iowa, Dept Phys & Astron, Iowa City, IA 52242 USA.
[Kar, P.; Kieda, D.; Smith, A. W.] Univ Utah, Dept Phys & Astron, Salt Lake City, UT 84112 USA.
[Kertzman, M.] Depauw Univ, Dept Phys & Astron, Greencastle, IN 46135 USA.
[McArthur, S.; Park, N.; Wakely, S. P.] Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA.
[McCann, A.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA.
[Meagher, K.; Otte, A. N.; Richards, G. T.] Georgia Inst Technol, Sch Phys, Atlanta, GA 30332 USA.
[Meagher, K.; Otte, A. N.; Richards, G. T.] Georgia Inst Technol, Ctr Relativist Astrophys, Atlanta, GA 30332 USA.
[Moriarty, P.] Galway Mayo Inst Technol, Dept Life & Phys Sci, Galway, Ireland.
[Mukherjee, R.] Columbia Univ Barnard Coll, Dept Phys & Astron, New York, NY 10027 USA.
[Nieto, D.] Columbia Univ, Dept Phys, New York, NY 10027 USA.
[Ong, R. A.; Popkow, A.] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA.
[Perkins, J. S.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Reyes, L. C.] Calif Polytech State Univ San Luis Obispo, Dept Phys, San Luis Obispo, CA 94307 USA.
[Reynolds, P. T.] Cork Inst Technol, Dept Appl Phys & Instrumentat, Bishopstown, Cork, Ireland.
RP Archer, A (reprint author), Washington Univ, Dept Phys, St Louis, MO 63130 USA.
EM beilicke@physics.wustl.edu
RI Khassen, Yerbol/I-3806-2015; Nieto, Daniel/J-7250-2015;
OI Khassen, Yerbol/0000-0002-7296-3100; Nieto, Daniel/0000-0003-3343-0755;
Pueschel, Elisa/0000-0002-0529-1973; Cui, Wei/0000-0002-6324-5772;
Barnacka, Anna/0000-0001-5655-4158; Lang, Mark/0000-0003-4641-4201;
Bird, Ralph/0000-0002-4596-8563
FU U.S. Department of Energy Office of Science; U.S. National Science
Foundation; Smithsonian Institution; NSERC in Canada; Science Foundation
Ireland [SFI 10/RFP/AST2748]; STFC in the UK
FX This research is supported by grants from the U.S. Department of Energy
Office of Science, the U.S. National Science Foundation, and the
Smithsonian Institution, by NSERC in Canada, by Science Foundation
Ireland (SFI 10/RFP/AST2748) and by STFC in the UK. We acknowledge the
excellent work of the technical support staff at the Fred Lawrence
Whipple Observatory and at the collaborating institutions in the
construction and operation of the instrument.
NR 61
TC 6
Z9 6
U1 1
U2 5
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 AUG 1
PY 2014
VL 790
IS 2
AR 149
DI 10.1088/0004-637X/790/2/149
PG 9
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AL4PV
UT WOS:000339115800066
ER
PT J
AU Bayliss, MB
Rigby, JR
Sharon, K
Wuyts, E
Florian, M
Gladders, MD
Johnson, T
Oguri, M
AF Bayliss, Matthew B.
Rigby, Jane R.
Sharon, Keren
Wuyts, Eva
Florian, Michael
Gladders, Michael D.
Johnson, Traci
Oguri, Masamune
TI THE PHYSICAL CONDITIONS, METALLICITY AND METAL ABUNDANCE RATIOS IN A
HIGHLY MAGNIFIED GALAXY AT z=3.6252
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: high-redshift; galaxies: star formation; gravitational
lensing: strong
ID STAR-FORMING GALAXIES; GRAVITATIONALLY LENSED GALAXY; STELLAR POPULATION
SYNTHESIS; LYMAN-BREAK GALAXY; GIANT ARCS SURVEY; SIMILAR-TO 2; INITIAL
MASS FUNCTION; DIGITAL SKY SURVEY; H-II REGIONS; ULTRAVIOLET-SPECTRUM
AB We present optical and near-IR imaging and spectroscopy of SGAS J105039.6+001730, a strongly lensed galaxy at z = 3.6252 magnified by >30x, and derive its physical properties. We measure a stellar mass of log(M-*/M-circle dot) = 9.5 +/- 0.35, star formation rates from [O II] lambda lambda 3727 and H beta of 55 +/- 25 and 84 +/- 24 M-circle dot yr(-1), respectively, an electron density of n(e) <= 10(3) cm(-2), an electron temperature of T-e <= 14,000 K, and a metallicity of 12 + log(O/H) = 8.3 +/- 0.1. The strong C III] lambda lambda 1907,1909 emission and abundance ratios of C, N, O, and Si are consistent with well-studied starbursts at z similar to 0 with similar metallicities. Strong P Cygni lines and He II lambda 1640 emission indicate a significant population of Wolf-Rayet stars, but synthetic spectra of individual populations of young, hot stars do not reproduce the observed integrated P Cygni absorption features. The rest-frame UV spectral features are indicative of a young starburst with high ionization, implying either (1) an ionization parameter significantly higher than suggested by rest-frame optical nebular lines, or (2) differences in one or both of the initial mass function and the properties of ionizing spectra of massive stars. We argue that the observed features are likely the result of a superposition of star forming regions with different physical properties. These results demonstrate the complexity of star formation on scales smaller than individual galaxies, and highlight the importance of systematic effects that result from smearing together the signatures of individual star forming regions within galaxies.
C1 [Bayliss, Matthew B.] Harvard Univ, Dept Phys, Cambridge, MA 02138 USA.
[Bayliss, Matthew B.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Rigby, Jane R.] NASA, Goddard Space Flight Ctr, Observat Cosmol Lab, Greenbelt, MD 20771 USA.
[Sharon, Keren; Johnson, Traci] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA.
[Wuyts, Eva] Max Planck Inst Extraterr Phys, D-85741 Garching, Germany.
[Florian, Michael; Gladders, Michael D.] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA.
[Florian, Michael; Gladders, Michael D.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA.
[Oguri, Masamune] Univ Tokyo, Dept Phys, Tokyo 1130033, Japan.
[Oguri, Masamune] Univ Tokyo, Kavli Inst Phys & Math Universe Kavli IPMU WPI, Chiba 2778583, Japan.
RP Bayliss, MB (reprint author), Harvard Univ, Dept Phys, 17 Oxford St, Cambridge, MA 02138 USA.
EM mbayliss@cfa.harvard.edu
RI Rigby, Jane/D-4588-2012; Oguri, Masamune/C-6230-2011
OI Rigby, Jane/0000-0002-7627-6551;
FU National Science Foundation [AST-1009012]; NASA from the Space Telescope
Science Institute [HST-GO-13003.01]; NASA [NAS5-26555]; JSPS [23740161];
FIRST program "Subaru Measurements of Images and Redshifts (SuMIRe),"
World Premier International Research Center Initiative (WPI Initiative),
MEXT, Japan
FX We thank Sally Heap and Dan Stark for interesting and helpful
discussions that improved this paper, as well as the anonymous referee
who provided very thoughtful and constructive feedback. This work was
supported by the National Science Foundation through grant AST-1009012,
by NASA through grant HST-GO-13003.01 from the Space Telescope Science
Institute, which is operated by the Association of Universities for
Research in Astronomy, Incorporated, under NASA contract NAS5-26555, and
also by the FIRST program "Subaru Measurements of Images and Redshifts
(SuMIRe)," World Premier International Research Center Initiative (WPI
Initiative), MEXT, Japan, and Grant-in-Aid for Scientific Research from
the JSPS (23740161).
NR 103
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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 AUG 1
PY 2014
VL 790
IS 2
AR 144
DI 10.1088/0004-637X/790/2/144
PG 20
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AL4PV
UT WOS:000339115800061
ER
PT J
AU Boyajian, TS
von Braun, K
van Belle, G
McAlister, HA
ten Brummelaar, TA
Kane, SR
Muirhead, PS
Jones, J
White, R
Schaefer, G
Ciardi, D
Henry, T
Lopez-Morales, M
Ridgway, S
Gies, D
Jao, WC
Rojas-Ayala, B
Parks, JR
Sturmann, L
Sturmann, J
Turner, NH
Farrington, C
Goldfinger, PJ
Berger, DH
AF Boyajian, Tabetha S.
von Braun, Kaspar
van Belle, Gerard
McAlister, Harold A.
ten Brummelaar, Theo A.
Kane, Stephen R.
Muirhead, Philip S.
Jones, Jeremy
White, Russel
Schaefer, Gail
Ciardi, David
Henry, Todd
Lopez-Morales, Mercedes
Ridgway, Stephen
Gies, Douglas
Jao, Wei-Chun
Rojas-Ayala, Barbara
Parks, J. Robert
Sturmann, Laszlo
Sturmann, Judit
Turner, Nils H.
Farrington, Chris
Goldfinger, P. J.
Berger, David H.
TI STELLAR DIAMETERS AND TEMPERATURES. II. MAIN-SEQUENCE K- AND M-STARS
(vol 757, pg 112, 2012)
SO ASTROPHYSICAL JOURNAL
LA English
DT Correction
ID LOW-MASS STARS; NEARBY RED DWARFS; INFRARED PHOTOMETRY; SOLAR
NEIGHBORHOOD; UBV PHOTOMETRY; STANDARD STARS; ECLIPSING BINARIES;
MAGNETIC ACTIVITY; UVBY PHOTOMETRY; BETA PHOTOMETRY
C1 [Boyajian, Tabetha S.; McAlister, Harold A.; Jones, Jeremy; White, Russel; Henry, Todd; Gies, Douglas; Jao, Wei-Chun; Rojas-Ayala, Barbara; Parks, J. Robert] Georgia State Univ, Ctr High Angular Resolut Astron, Atlanta, GA 30302 USA.
[Boyajian, Tabetha S.; McAlister, Harold A.; Jones, Jeremy; White, Russel; Henry, Todd; Gies, Douglas; Jao, Wei-Chun; Parks, J. Robert] Georgia State Univ, Dept Phys & Astron, Atlanta, GA 30302 USA.
[von Braun, Kaspar; Kane, Stephen R.; Ciardi, David] CALTECH, NASA, Exoplanet Sci Inst, Pasadena, CA 91125 USA.
[van Belle, Gerard] Lowell Observ, Flagstaff, AZ 86001 USA.
[ten Brummelaar, Theo A.; Schaefer, Gail; Sturmann, Laszlo; Sturmann, Judit; Turner, Nils H.; Farrington, Chris; Goldfinger, P. J.] Mt Wilson Observ, CHARA Array, Mount Wilson, CA 91023 USA.
[Muirhead, Philip S.] CALTECH, Dept Astron, Pasadena, CA 91125 USA.
[Lopez-Morales, Mercedes] CSIC, IEEC, Inst Ciencies Espai, E-08193 Barcelona, Spain.
[Lopez-Morales, Mercedes] Carnegie Inst Sci, Dept Terr Magnetism, Washington, DC 20015 USA.
[Ridgway, Stephen] Natl Opt Astron Observ, Tucson, AZ 85726 USA.
[Rojas-Ayala, Barbara] Amer Museum Nat Hist, Dept Astrophys, Div Phys Sci, New York, NY 10024 USA.
[Berger, David H.] Syst Planning Corp, Arlington, VA 22201 USA.
RP Boyajian, TS (reprint author), Georgia State Univ, Ctr High Angular Resolut Astron, POB 4106, Atlanta, GA 30302 USA.
RI Rojas-Ayala, Barbara/G-4382-2015; Muirhead, Philip/H-2273-2014;
OI Rojas-Ayala, Barbara/0000-0002-0149-1302; Muirhead,
Philip/0000-0002-0638-8822; Boyajian, Tabetha/0000-0001-9879-9313
NR 217
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U1 1
U2 4
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 AUG 1
PY 2014
VL 790
IS 2
AR 166
DI 10.1088/0004-637X/790/2/166
PG 4
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AL4PV
UT WOS:000339115800083
ER
PT J
AU Brosius, JW
Daw, AN
Rabin, DM
AF Brosius, Jeffrey W.
Daw, Adrian N.
Rabin, D. M.
TI PERVASIVE FAINT Fe XIX EMISSION FROM A SOLAR ACTIVE REGION OBSERVED WITH
EUNIS-13: EVIDENCE FOR NANOFLARE HEATING
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE Sun: activity; Sun: corona; Sun: flares; Sun: UV radiation
ID CORONAL DIAGNOSTIC SPECTROMETER; EXTREME-ULTRAVIOLET SPECTRUM; HIGH TIME
RESOLUTION; X-RAY TELESCOPE; HOT PLASMA; CHROMOSPHERIC EVAPORATION;
RESONANT ABSORPTION; SOUNDING ROCKET; ATOMIC DATABASE; ENERGY-RELEASE
AB We present spatially resolved EUV spectroscopic measurements of pervasive, faint Fe XIX 592.2 angstrom line emission in an active region observed during the 2013 April 23 flight of the Extreme Ultraviolet Normal Incidence Spectrograph (EUNIS-13) sounding rocket instrument. With cooled detectors, high sensitivity, and high spectral resolution, EUNIS-13 resolves the lines of Fe XIX at 592.2 angstrom(formed at temperature T approximate to 8.9MK) and Fe XII at 592.6 angstrom (T approximate to 1.6MK). The Fe XIX line emission, observed over an area in excess of 4920 arcsec(2) (2.58 x 10(9) km(2), more than 60% of the active region), provides strong evidence for the nanoflare heating model of the solar corona. No GOES events occurred in the region less than 2 hr before the rocket flight, but a microflare was observed north and east of the region with RHESSI and EUNIS during the flight. The absence of significant upward velocities anywhere in the region, particularly the microflare, indicates that the pervasive Fe XIX emission is not propelled outward from the microflare site, but is most likely attributed to localized heating (not necessarily due to reconnection) consistent with the nanoflare heating model of the solar corona. Assuming ionization equilibrium we estimate Fe XIX/Fe XII emission measure ratios of similar to 0.076 just outside the AR core and similar to 0.59 in the core.
C1 [Brosius, Jeffrey W.] Catholic Univ Amer, NASA, Goddard Space Flight Ctr, Solar Phys Lab, Greenbelt, MD 20771 USA.
[Daw, Adrian N.] NASA, Goddard Space Flight Ctr, Solar Phys Lab, Greenbelt, MD 20771 USA.
[Rabin, D. M.] NASA, Goddard Space Flight Ctr, Heliophys Sci Div, Greenbelt, MD 20771 USA.
RP Brosius, JW (reprint author), Catholic Univ Amer, NASA, Goddard Space Flight Ctr, Solar Phys Lab, Code 671, Greenbelt, MD 20771 USA.
EM Jeffrey.W.Brosius@nasa.gov
FU NASA Heliophysics Division through its Low Cost Access to Space program
FX EUNIS-13 was supported by the NASA Heliophysics Division through its Low
Cost Access to Space program. CHIANTI is a collaborative project
involving George Mason University, the University of Michigan (USA), and
the University of Cambridge (UK). We thank Dr. Gordon Holman for
assistance with creating the RHESSI image, and the anonymous referee for
valuable comments that helped improve the manuscript.
NR 68
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U1 1
U2 2
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 AUG 1
PY 2014
VL 790
IS 2
AR 112
DI 10.1088/0004-637X/790/2/112
PG 8
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AL4PV
UT WOS:000339115800029
ER
PT J
AU Desjardins, TD
Gallagher, SC
Hornschemeier, AE
Mulchaey, JS
Walker, LM
Brandt, WN
Charlton, JC
Johnson, KE
Tzanavaris, P
AF Desjardins, Tyler D.
Gallagher, Sarah C.
Hornschemeier, Ann E.
Mulchaey, John S.
Walker, Lisa May
Brandt, William N.
Charlton, Jane C.
Johnson, Kelsey E.
Tzanavaris, Panayiotis
TI SOME LIKE IT HOT: LINKING DIFFUSE X-RAY LUMINOSITY, BARYONIC MASS, AND
STAR FORMATION RATE IN COMPACT GROUPS OF GALAXIES
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: groups: general; X-rays: galaxies
ID CHANDRA MULTIWAVELENGTH PROJECT; NORMAL ELLIPTIC GALAXIES; NORTH POLAR
SPUR; SPECTRAL ENERGY-DISTRIBUTIONS; NEAR-INFRARED PROPERTIES; ACTIVE
GALACTIC NUCLEUS; ALL-SKY SURVEY; REDSHIFT SURVEY; INTERSTELLAR-MEDIUM;
SCALING RELATIONS
AB We present an analysis of the diffuse X-ray emission in 19 compact groups (CGs) of galaxies observed with Chandra. The hottest, most X-ray luminous CGs agree well with the galaxy cluster X-ray scaling relations in L-X-T and L-X-sigma, even in CGs where the hot gas is associated with only the brightest galaxy. Using Spitzer photometry, we compute stellar masses and classify Hickson CGs 19, 22, 40, and 42, and RSCGs 32, 44, and 86 as fossil groups using a new definition for fossil systems that includes a broader range of masses. We find that CGs with total stellar and Hi masses greater than or similar to 10(11.3) M-circle dot are often X-ray luminous, while lower-mass CGs only sometimes exhibit faint, localized X-ray emission. Additionally, we compare the diffuse X-ray luminosity against both the total UV and 24 m star formation rates of each CG and optical colors of the most massive galaxy in each of the CGs. The most X-ray luminous CGs have the lowest star formation rates, likely because there is no cold gas available for star formation, either because the majority of the baryons in these CGs are in stars or the X-ray halo, or due to gas stripping from the galaxies in CGs with hot halos. Finally, the optical colors that trace recent star formation histories of the most massive group galaxies do not correlate with the X-ray luminosities of the CGs, indicating that perhaps the current state of the X-ray halos is independent of the recent history of stellar mass assembly in the most massive galaxies.
C1 [Desjardins, Tyler D.; Gallagher, Sarah C.] Univ Western Ontario, Dept Phys & Astron, London, ON N6A 3K7, Canada.
[Hornschemeier, Ann E.; Tzanavaris, Panayiotis] NASA, Goddard Space Flight Ctr, Lab Xray Astrophys, Greenbelt, MD 20771 USA.
[Mulchaey, John S.] Carnegie Observ, Pasadena, CA 91101 USA.
[Walker, Lisa May; Johnson, Kelsey E.] Univ Virginia, Dept Astron, Charlottesville, VA 22904 USA.
[Brandt, William N.; Charlton, Jane C.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA.
[Tzanavaris, Panayiotis] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA.
RP Desjardins, TD (reprint author), Univ Western Ontario, Dept Phys & Astron, London, ON N6A 3K7, Canada.
RI Brandt, William/N-2844-2015
OI Brandt, William/0000-0002-0167-2453
FU Natural Science and Engineering Research Council of Canada; Ontario
Early Researcher Award Program; NASA ADP grant [NNX10AC99G]; NSF grant
[AST-1108604]; NSF [AST-0908984]; ACIS [SAO SV4-74018]; Alfred P. Sloan
Foundation; National Science Foundation; U.S. Department of Energy
Office of Science
FX T.D.D. and S.C.G. thank the Natural Science and Engineering Research
Council of Canada and the Ontario Early Researcher Award Program for
support. W.N.B. is supported by NASA ADP grant NNX10AC99G and NSF grant
AST-1108604 for support. J.C.C. thanks NSF for funding under award
AST-0908984. This work was partially supported by the ACIS Instrument
Team contract SAO SV4-74018 (PI: G. Garmire). 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. Based
on observations obtained with the Apache Point Observatory 3.5 m
telescope, which is owned and operated by the Astrophysical Research
Consortium. Funding for SDSS-III has been provided by the Alfred P.
Sloan Foundation, the Participating Institutions, the National Science
Foundation, and the U.S. Department of Energy Office of Science. The
SDSS-III Web site is http://www.sdss3.org/.
NR 141
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U1 1
U2 2
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 AUG 1
PY 2014
VL 790
IS 2
AR 132
DI 10.1088/0004-637X/790/2/132
PG 15
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AL4PV
UT WOS:000339115800049
ER
PT J
AU Fabrycky, DC
Lissauer, JJ
Ragozzine, D
Rowe, JF
Steffen, JH
Agol, E
Barclay, T
Batalha, N
Borucki, W
Ciardi, DR
Ford, EB
Gautier, TN
Geary, JC
Holman, MJ
Jenkins, JM
Li, J
Morehead, RC
Morris, RL
Shporer, A
Smith, JC
Still, M
Van Cleve, J
AF Fabrycky, Daniel C.
Lissauer, Jack J.
Ragozzine, Darin
Rowe, Jason F.
Steffen, Jason H.
Agol, Eric
Barclay, Thomas
Batalha, Natalie
Borucki, William
Ciardi, David R.
Ford, Eric B.
Gautier, Thomas N.
Geary, John C.
Holman, Matthew J.
Jenkins, Jon M.
Li, Jie
Morehead, Robert C.
Morris, Robert L.
Shporer, Avi
Smith, Jeffrey C.
Still, Martin
Van Cleve, Jeffrey
TI ARCHITECTURE OF KEPLER'S MULTI-TRANSITING SYSTEMS. II. NEW
INVESTIGATIONS WITH TWICE AS MANY CANDIDATES
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE methods: statistical; planetary systems; planets and satellites:
detection; planets and satellites: dynamical evolution and stability
ID PLANET SYSTEMS; ORBITAL ECCENTRICITIES; MULTIPLANET SYSTEMS; TIMING
OBSERVATIONS; SUPER-EARTH; DYNAMICS; CONFIRMATION; STABILITY; MIGRATION;
HARPS
AB We report on the orbital architectures of Kepler systems having multiple-planet candidates identified in the analysis of data from the first six quarters of Kepler data and reported by Batalha et al. (2013). These data show 899 transiting planet candidates in 365 multiple-planet systems and provide a powerful means to study the statistical properties of planetary systems. Using a generic mass-radius relationship, we find that only two pairs of planets in these candidate systems (out of 761 pairs total) appear to be on Hill-unstable orbits, indicating similar to 96% of the candidate planetary systems are correctly interpreted as true systems. We find that planet pairs show little statistical preference to be near mean-motion resonances. We identify an asymmetry in the distribution of period ratios near first-order resonances (e.g., 2:1, 3:2), with an excess of planet pairs lying wide of resonance and relatively few lying narrow of resonance. Finally, based upon the transit duration ratios of adjacent planets in each system, we find that the interior planet tends to have a smaller transit impact parameter than the exterior planet does. This finding suggests that the mode of the mutual inclinations of planetary orbital planes is in the range 1 degrees.0-2 degrees.2, for the packed systems of small planets probed by these observations.
C1 [Fabrycky, Daniel C.] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA.
[Lissauer, Jack J.; Rowe, Jason F.; Barclay, Thomas; Batalha, Natalie; Borucki, William; Jenkins, Jon M.; Li, Jie; Morris, Robert L.; Smith, Jeffrey C.; Van Cleve, Jeffrey] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Ragozzine, Darin; Geary, John C.; Holman, Matthew J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Rowe, Jason F.; Li, Jie; Morris, Robert L.; Smith, Jeffrey C.; Van Cleve, Jeffrey] SETI Inst, Mountain View, CA 94043 USA.
[Steffen, Jason H.] Fermilab Ctr Particle Astrophys, Batavia, IL 60510 USA.
[Steffen, Jason H.] CIERA Northwestern Univ, Evanston, IL 60208 USA.
[Agol, Eric] Univ Washington, Dept Astron, Seattle, WA 98195 USA.
[Barclay, Thomas; Still, Martin] NASA, Ames Res Ctr, Bay Area Environm Res Inst, Moffett Field, CA 94035 USA.
[Batalha, Natalie] San Jose State Univ, Dept Phys & Astron, San Jose, CA 95192 USA.
[Ciardi, David R.] CALTECH, NASA, Exoplanet Sci Inst, Pasadena, CA 91125 USA.
[Ford, Eric B.; Morehead, Robert C.] Penn State Univ, Davey Lab 525, Ctr Exoplanets & Habitable Worlds, University Pk, PA 16802 USA.
[Ford, Eric B.; Morehead, Robert C.] Penn State Univ, Davey Lab 525, Dept Astron & Astrophys, University Pk, PA 16802 USA.
[Ford, Eric B.; Morehead, Robert C.] Univ Florida, Dept Astron, Gainesville, FL 32111 USA.
[Gautier, Thomas N.; Shporer, Avi] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Shporer, Avi] Las Cumbres Observ Global Telescope Network, Santa Barbara, CA 93117 USA.
[Shporer, Avi] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA.
RP Fabrycky, DC (reprint author), Univ Chicago, Dept Astron & Astrophys, 5640 S Ellis Ave, Chicago, IL 60637 USA.
EM fabrycky@uchicago.edu
OI /0000-0002-0802-9145; Ciardi, David/0000-0002-5741-3047;
/0000-0001-6545-639X; Fabrycky, Daniel/0000-0003-3750-0183
FU NASA's Science Mission Directorate; NASA through Hubble Fellowship
[HF-51272.01-A]; NASA [NAS 5-26555]; NSF [0645416]; National Aeronautics
and Space Administration [NNX08AR04G]; Pennsylvania State University;
Eberly College of Science; Pennsylvania Space Grant Consortium; National
Science Foundation [0707203, DGE-0802270]
FX Funding for this mission is provided by NASA's Science Mission
Directorate. We thank the entire Kepler team for the many years of work
that is making the Kepler mission so successful. We thank Emily
Fabrycky, Doug Lin, Man-Hoi Lee, Scott Tremaine, and Tsevi Mazeh for
helpful conversations and insightful comments. D.C F. acknowledges
support for this work was provided by NASA through Hubble Fellowship
grant No. HF-51272.01-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. E.A.
was supported by NSF Career grant 0645416. E.B.F acknowledges support by
the National Aeronautics and Space Administration under grant NNX08AR04G
issued through the Kepler Participating Scientist Program, and the
Center for Exoplanets and Habitable Worlds, which is supported by the
Pennsylvania State University, the Eberly College of Science, and the
Pennsylvania Space Grant Consortium. This material is based upon work
supported by the National Science Foundation under grant No. 0707203.
R.C.M. was support by the National Science Foundation Graduate Research
Fellowship under grant No. DGE-0802270.
NR 40
TC 107
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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
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD AUG 1
PY 2014
VL 790
IS 2
AR 146
DI 10.1088/0004-637X/790/2/146
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AL4PV
UT WOS:000339115800063
ER
PT J
AU Farnocchia, D
Chesley, SR
Chodas, PW
Tricarico, P
Kelley, MSP
Farnham, TL
AF Farnocchia, Davide
Chesley, Steven R.
Chodas, Paul W.
Tricarico, Pasquale
Kelley, Michael S. P.
Farnham, Tony L.
TI TRAJECTORY ANALYSIS FOR THE NUCLEUS AND DUST OF COMET C/2013 A1 (SIDING
SPRING)
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE celestial mechanics; comets: individual (C/2013 A1); methods:
analytical; radiation: dynamics
ID MARS; FORCES
AB Comet C/2013 A1 (Siding Spring) will experience a high velocity encounter with Mars on 2014 October 19 at a distance of 135,000 km +/- 5000 km from the planet center. We present a comprehensive analysis of the trajectory of both the comet nucleus and the dust tail. The nucleus of C/2013 A1 cannot impact on Mars even in the case of unexpectedly large nongravitational perturbations. Furthermore, we compute the required ejection velocities for the dust grains of the tail to reach Mars as a function of particle radius and density and heliocentric distance of the ejection. A comparison between our results and the most current modeling of the ejection velocities suggests that impacts are possible only for millimeter to centimeter size particles released more than 13AU from the Sun. However, this level of cometary activity that far from the Sun is considered extremely unlikely. The arrival time of these particles spans a 20-minute time interval centered at 2014 October 19 at 20: 09 TDB, i.e., around the time that Mars crosses the orbital plane of C/2013 A1. Ejection velocities larger than currently estimated by a factor >2 would allow impacts for smaller particles ejected as close as 3AU from the Sun. These particles would reach Mars from 19:13 TDB to 20:40 TDB.
C1 [Farnocchia, Davide; Chesley, Steven R.; Chodas, Paul W.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Tricarico, Pasquale] Planetary Sci Inst, Tucson, AZ 85719 USA.
[Kelley, Michael S. P.; Farnham, Tony L.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
RP Farnocchia, D (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
EM Davide.Farnocchia@jpl.nasa.gov
OI Kelley, Michael/0000-0002-6702-7676; Chesley, Steven/0000-0003-3240-6497
NR 15
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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 AUG 1
PY 2014
VL 790
IS 2
AR 114
DI 10.1088/0004-637X/790/2/114
PG 7
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AL4PV
UT WOS:000339115800031
ER
PT J
AU Fuskeland, U
Wehus, IK
Eriksen, HK
Naess, SK
AF Fuskeland, U.
Wehus, I. K.
Eriksen, H. K.
Naess, S. K.
TI SPATIAL VARIATIONS IN THE SPECTRAL INDEX OF POLARIZED SYNCHROTRON
EMISSION IN THE 9 yr WMAP SKY MAPS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE cosmic background radiation; cosmology: observations; Galaxy: structure;
methods: statistical; polarization; radio continuum: general
ID COMPONENT SEPARATION; MICROWAVE; POWER
AB We estimate the spectral index, beta, of polarized synchrotron emission as observed in the 9 yr Wilkinson Microwave Anisotropy Probe sky maps using two methods, linear regression ("T-T plot") and maximum likelihood. We partition the sky into 24 disjoint sky regions and evaluate the spectral index for all polarization angles between 0. and 85 degrees in steps of 5 degrees. Averaging over polarization angles, we derive a mean spectral index of beta(all-sky) = -2.99 +/- 0.01 in the frequency range of 23-33 GHz. We find that the synchrotron spectral index steepens by 0.14 from low to high Galactic latitudes, in agreement with previous studies, with mean spectral indices of beta(plane) = -2.98 +/- 0.01 and beta(high-lat) = -3.12 +/- 0.04. In addition, we find a significant longitudinal variation along the Galactic plane with a steeper spectral index toward the Galactic center and anticenter than toward the Galactic spiral arms. This can be well modeled by an offset sinusoidal, beta(l) = -2.85 + 0.17 sin(2l - 90 degrees). Finally, we study synchrotron emission in the BICEP2 field, in an attempt to understand whether the claimed detection of large-scale B-mode polarization could be explained in terms of synchrotron contamination. Adopting a spectral index of beta = -3.12, typical for high Galactic latitudes, we find that the most likely bias corresponds to about 2% of the reported signal (r = 0.003). The flattest index allowed by the data in this region is beta = -2.5, and under the assumption of a straight power-law frequency spectrum, we find that synchrotron emission can account for at most 20% of the reported BICEP2 signal.
C1 [Fuskeland, U.; Eriksen, H. K.; Naess, S. K.] Univ Oslo, Inst Theoret Astrophys, NO-0315 Oslo, Norway.
[Wehus, I. K.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Wehus, I. K.; Naess, S. K.] Univ Oxford, DWB, Oxford OX1 3RH, England.
RP Fuskeland, U (reprint author), Univ Oslo, Inst Theoret Astrophys, POB 1029 Blindern, NO-0315 Oslo, Norway.
EM unnif@astro.uio.no; i.k.wehus@fys.uio.no; h.k.k.eriksen@astro.uio.no;
s.k.nass@astro.uio.no
FU ERC [StG2010-257080, 259505]; NASA
FX The computations presented in this paper were carried out on Abel, a
cluster owned and maintained by the University of Oslo and NOTUR. This
project was supported by the ERC Starting Grant StG2010-257080. I. K. W.
acknowledges support from ERC grant 259505. Part of the research was
carried out at the Jet Propulsion Laboratory, California Institute of
Technology, under a contract with NASA. Some of the results in this
paper have been derived using the HEALPix (Gorski et al. 2005) software
and analysis package.
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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 AUG 1
PY 2014
VL 790
IS 2
AR 104
DI 10.1088/0004-637X/790/2/104
PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AL4PV
UT WOS:000339115800021
ER
PT J
AU Gatuzz, E
Garcia, J
Mendoza, C
Kallman, TR
Bautista, MA
Gorczyca, TW
AF Gatuzz, E.
Garcia, J.
Mendoza, C.
Kallman, T. R.
Bautista, M. A.
Gorczyca, T. W.
TI PHYSICAL PROPERTIES OF THE INTERSTELLAR MEDIUM USING HIGH-RESOLUTION
CHANDRA SPECTRA: O K-EDGE ABSORPTION
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE atomic processes; ISM: abundances; ISM: atoms; X-rays: binaries; X-rays:
ISM
ID X-RAY SPECTROSCOPY; XMM-NEWTON OBSERVATION; NEUTRON-STAR; ATOMIC OXYGEN;
SCORPIUS X-1; 4U 1820-30; CYG X-2; SHELL PHOTOABSORPTION;
CROSS-SECTIONS; LOW/HARD STATE
AB Chandra high-resolution spectra toward eight low-mass Galactic binaries have been analyzed with a photoionization model that is capable of determining the physical state of the interstellar medium. Particular attention is given to the accuracy of the atomic data. Hydrogen column densities are derived with a broadband fit that takes into account pileup effects, and in general are in good agreement with previous results. The dominant features in the oxygen-edge region are OI and OII K alpha absorption lines whose simultaneous fits lead to average values of the ionization parameter of log xi = -2.90 and oxygen abundance of A(O) = 0.70. The latter is given relative to the standard by Grevesse & Sauval, but rescaling with the revision by Asplund et al. would lead to an average abundance value fairly close to solar. The low average oxygen column density (N-O = 9.2 x 10(17) cm(-2)) suggests a correlation with the low ionization parameters, the latter also being in evidence in the column density ratios N(O II)/N(O I) and N(O III)/N(O I) that are estimated to be less than 0.1. We do not find conclusive evidence for absorption by any other compound but atomic oxygen in our oxygen-edge region analysis.
C1 [Gatuzz, E.; Mendoza, C.] Inst Venezolano Invest Cient, Ctr Fis, Caracas 1020A, Venezuela.
[Garcia, J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Mendoza, C.; Bautista, M. A.; Gorczyca, T. W.] Western Michigan Univ, Dept Phys, Kalamazoo, MI 49008 USA.
[Kallman, T. R.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Gatuzz, E (reprint author), Inst Venezolano Invest Cient, Ctr Fis, POB 20632, Caracas 1020A, Venezuela.
EM egatuzz@ivic.gob.ve; javier@head.cfa.harvard.edu; claudio@ivic.gob.ve;
timothy.r.kallman@nasa.gov; manuel.bautista@wmich.edu;
thomas.gorczyca@wmich.edu
OI Mendoza, Claudio/0000-0002-2854-4806
FU National Science Foundation [AST-1313265]
FX Part of this work was carried out by Efrain Gatuzz during a visit in
2014 January to the Laboratory of High Energy Astrophysics, NASA Goddard
Space Flight Center, Greenbelt, Maryland, USA. Their hospitality and
financial support are gratefully acknowledged. Manuel Bautista has
received financial support from the National Science Foundation through
grant AST-1313265. We would also like to thank Dr. Frits Paerels for
comments at the refereeing stage that led to substantial improvements of
the arguments presented and thus of the final quality of the paper.
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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 AUG 1
PY 2014
VL 790
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AR 131
DI 10.1088/0004-637X/790/2/131
PG 11
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AL4PV
UT WOS:000339115800048
ER
PT J
AU Kassin, SA
Brooks, A
Governato, F
Weiner, BJ
Gardner, JP
AF Kassin, Susan A.
Brooks, Alyson
Governato, Fabio
Weiner, Benjamin J.
Gardner, Jonathan P.
TI KINEMATIC EVOLUTION OF SIMULATED STAR-FORMING GALAXIES
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: evolution; galaxies: formation; galaxies: fundamental
parameters; galaxies: kinematics and dynamics; galaxies: spiral
ID COSMOLOGICAL ZOOM SIMULATIONS; INITIAL MASS FUNCTION; TULLY-FISHER
RELATION; NEARBY GALAXIES; STELLAR FEEDBACK; FORMATION LAW; HYDRODYNAMIC
SIMULATIONS; PHYSICAL-PROPERTIES; MOLECULAR-HYDROGEN; DWARF GALAXIES
AB Recent observations have shown that star-forming galaxies like our own Milky Way evolve kinematically into ordered thin disks over the last similar to 8 billion years since z = 1.2, undergoing a process of "disk settling." For the first time, we study the kinematic evolution of a suite of four state of the art "zoom in" hydrodynamic simulations of galaxy formation and evolution in a fully cosmological context and compare with these observations. Until now, robust measurements of the internal kinematics of simulated galaxies were lacking because the simulations suffered from low resolution, overproduction of stars, and overly massive bulges. The current generation of simulations has made great progress in overcoming these difficulties and is ready for a kinematic analysis. We show that simulated galaxies follow the same kinematic trends as real galaxies: they progressively decrease in disordered motions (sigma(g)) and increase in ordered rotation (V-rot) with time. The slopes of the relations between both sigma(g) and V-rot with redshift are consistent between the simulations and the observations. In addition, the morphologies of the simulated galaxies become less disturbed with time, also consistent with observations. This match between the simulated and observed trends is a significant success for the current generation of simulations, and a first step in determining the physical processes behind disk settling.
C1 [Kassin, Susan A.] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
[Brooks, Alyson] Rutgers State Univ, Dept Phys & Astron, Piscataway, NJ 08854 USA.
[Governato, Fabio] Univ Washington, Dept Astron, Seattle, WA 98195 USA.
[Weiner, Benjamin J.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA.
[Gardner, Jonathan P.] Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA.
RP Kassin, SA (reprint author), Space Telescope Sci Inst, 3700 San Martin Dr, Baltimore, MD 21218 USA.
EM kassin@stsci.edu
OI Kassin, Susan/0000-0002-3838-8093
FU NSF [AST-0607819]; NASA High-End Computing (HEC) Program through the
NASA Advanced Supercomputing (NAS) Division at Ames Research Center
FX F.G. acknowledges support from NSF grant AST-0607819. 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. A.B. thanks Jay Gallagher for helpful conversations.
NR 54
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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 AUG 1
PY 2014
VL 790
IS 2
AR 89
DI 10.1088/0004-637X/790/2/89
PG 5
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AL4PV
UT WOS:000339115800006
ER
PT J
AU Mahapatra, DP
Chutjian, A
Machacek, JR
Mangina, RS
AF Mahapatra, D. P.
Chutjian, A.
Machacek, J. R.
Mangina, R. S.
TI SIZE DISTRIBUTION OF POSSIBLE DUST CARRIERS FOR THE EXTENDED RED
EMISSION
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE dust, extinction
ID AROMATIC-HYDROCARBON CLUSTERS; SILICON NANOPARTICLES; BLUE LUMINESCENCE;
INTERSTELLAR-MEDIUM; GRAINS; INJECTION; RECTANGLE; NGC-7023; SYSTEM
AB Power-law size distributions expected to be applicable to possible carriers of extended red emission (ERE) have been examined using Monte Carlo (MC) simulations. Si nanoparticles and some polycyclic aromatic hydrocarbon complexes such as oligoacene and oligorylenes with energy gaps close to 2 eV have been considered. In the simplest case of unit quantum efficiency, the MC-generated size distributions are used to obtain photoluminescence (PL) spectra that are then corrected for dust extinction and reddening effects for comparison with observed ERE spectra. It is shown that a power-law size distribution with a decay exponent of alpha = 7/2, which closely agrees with starlight extinction data, fails to produce an ERE-like spectrum. However, size distributions with decay exponents of alpha = 19/12 and 3/2 are found to lead to acceptable spectra. Results indicate that energetic photon-induced breakup and competing aggregation effects dominate collisional effects in producing the observed steady-statemass distribution. It is shown that the peak wavelength of emission critically depends on the band gap, rather than cluster mass, which for oligoacenes and oligorylenes is widely different. The peak wavelength is also shown to be insensitive to dust attenuation.
C1 [Mahapatra, D. P.; Chutjian, A.; Machacek, J. R.; Mangina, R. S.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Mahapatra, DP (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
EM ara.chutjian@jpl.nasa.gov
RI Machacek, Joshua/A-5316-2011
FU NASA through the NASA Senior Research Associate Program
FX We thank M. P. Das for helpful discussions. D.P.M. acknowledges support
from NASA through the NASA Senior Research Associate Program managed by
the Oak Ridge Associated Universities, USA. This research was carried
out at JPL/Caltech under contract with the National Aeronautics and
Space Administration.
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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 AUG 1
PY 2014
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DI 10.1088/0004-637X/790/2/140
PG 5
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AL4PV
UT WOS:000339115800057
ER
PT J
AU Ressler, SM
Katsuda, S
Reynolds, SP
Long, KS
Petre, R
Williams, BJ
Winkler, PF
AF Ressler, Sean M.
Katsuda, Satoru
Reynolds, Stephen P.
Long, Knox S.
Petre, Robert
Williams, Brian J.
Winkler, P. Frank
TI MAGNETIC FIELD AMPLIFICATION IN THE THIN X-RAY RIMS OF SN 1006
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE acceleration of particles; ISM: individual objects (SN 1006); ISM:
magnetic fields; ISM: supernova remnants; X-rays: ISM
ID YOUNG SUPERNOVA-REMNANTS; DIFFUSIVE SHOCK ACCELERATION; SMALL-SCALE
STRUCTURE; PARTICLE-ACCELERATION; SYNCHROTRON EMISSION; CHANDRA
OBSERVATIONS; NORTHEASTERN LIMB; MAXIMUM ENERGY; CASSIOPEIA-A; FILAMENTS
AB Several young supernova remnants, including SN 1006, emit synchrotron X-rays in narrow filaments, hereafter thin rims, along their periphery. The widths of these rims imply 50-100 G fields in the region immediately behind the shock, far larger than expected for the interstellar medium compressed by unmodified shocks, assuming electron radiative losses limit rim widths. However, magnetic field damping could also produce thin rims. Here we review the literature on rim width calculations, summarizing the case for magnetic field amplification. We extend these calculations to include an arbitrary power-law dependence of the diffusion coefficient on energy, D. E. Loss-limited rim widths should shrink with increasing photon energy, while magnetic-damping models predict widths almost independent of photon energy. We use these results to analyze Chandra observations of SN 1006, in particular the southwest limb. We parameterize the FWHM in terms of energy as FWHM alpha E-nu(mE) Filament widths in SN 1006 decrease with energy; m(E) similar to -0.3 to -0.8, implying magnetic field amplification by factors of 10-50, above the factor of four expected in strong unmodified shocks. For SN 1006, the rapid shrinkage rules out magnetic damping models. It also favors short mean free paths (small diffusion coefficients) and strong dependence of D on energy (mu >= 1).
C1 [Ressler, Sean M.] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA.
[Katsuda, Satoru] Japan Aerosp Explorat Agcy JAXA, Inst Space & Astronaut Sci, Sagamihara, Kanagawa 2525210, Japan.
[Reynolds, Stephen P.] N Carolina State Univ, Dept Phys, Raleigh, NC 27695 USA.
[Long, Knox S.] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
[Petre, Robert; Williams, Brian J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Winkler, P. Frank] Middlebury Coll, Dept Phys, Middlebury, VT 05753 USA.
RP Ressler, SM (reprint author), Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA.
FU National Aeronautics and Space Administration through Chandra grant by
the Chandra X-Ray Observatory Center [GO2-13066]; NASA [NAS8-03060]
FX Support for this work was provided by the National Aeronautics and Space
Administration through Chandra grant Number GO2-13066, issued by the
Chandra X-Ray Observatory Center, which is operated by the Smithsonian
Astrophysical Observatory for and on behalf of NASA under contract
NAS8-03060.
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SN 0004-637X
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J9 ASTROPHYS J
JI Astrophys. J.
PD AUG 1
PY 2014
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SC Astronomy & Astrophysics
GA AL4PV
UT WOS:000339115800002
ER
PT J
AU Veilleux, S
Teng, SH
Rupke, DSN
Maiolino, R
Sturm, E
AF Veilleux, S.
Teng, S. H.
Rupke, D. S. N.
Maiolino, R.
Sturm, E.
TI HALF-MEGASECOND CHANDRA SPECTRAL IMAGING OF THE HOT CIRCUMGALACTIC
NEBULA AROUND QUASAR MRK 231
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: active; galaxies: starburst; ISM: jets and outflows; quasars:
individual (Mrk 231); X-rays: galaxies
ID ULTRALUMINOUS INFRARED GALAXIES; X-RAY-EMISSION; ABSORPTION-LINE QUASAR;
MERGER NGC 6240; XMM-NEWTON; INTERSTELLAR-MEDIUM; MOLECULAR OUTFLOWS;
ELLIPTIC GALAXIES; STAR-FORMATION; CHEMICAL ENRICHMENT
AB A deep 400 ks ACIS-S observation of the nearest quasar known, Mrk 231, is combined with archival 120 ks data to carry out the first ever spatially resolved spectral analysis of a hot X-ray-emitting circumgalactic nebula around a quasar. The 65 x 50 kpc X-ray nebula shares no resemblance with the tidal debris seen at optical wavelengths. One notable exception is the small tidal arc similar to 3.5 kpc south of the nucleus where excess soft X-ray continuum emission and Si XIII 1.8 keV line emission are detected, consistent with star formation and its associated alpha-element enhancement, respectively. An X-ray shadow is also detected at the location of the 15 kpc northern tidal tail. The hard X-ray continuum emission within similar to 6 kpc of the center is consistent with being due entirely to the bright central active galactic nucleus. The soft X-ray spectrum of the outer (greater than or similar to 6 kpc) portion of the nebula is best described as the sum of two thermal components with temperatures similar to 3 and similar to 8 million K and spatially uniform super-solar alpha-element abundances, relative to iron. This result implies enhanced star formation activity over similar to 10(8) yr, accompanied by redistribution of the metals on a large scale. The low-temperature thermal component is not present within similar to 6 kpc of the nucleus, suggesting extra heating in this region from the circumnuclear starburst, the central quasar, or the optically identified greater than or similar to 3 kpc quasar-driven outflow. The soft X-ray emission is weaker in the western quadrant, coincident with a deficit of H alpha and some of the largest columns of neutral gas outflowing from the nucleus. Shocks may heat the gas to high temperatures at this location, consistent with the tentative similar to 2 sigma detection of extended Fe XXV 6.7 keV line emission.
C1 [Veilleux, S.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Veilleux, S.] Univ Maryland, Joint Space Sci Inst, College Pk, MD 20742 USA.
[Teng, S. H.] NASA Goddard Space Flight Ctr, Observat Cosmol Lab, Greenbelt, MD 20771 USA.
[Rupke, D. S. N.] Dept Phys, Rhodes Coll, Memphis, TN 38112 USA.
[Maiolino, R.] Univ Cambridge, Cavendish Lab, Cambridge CB3 0HE, England.
[Maiolino, R.] Kavli Inst Cosmol, Cambridge CB3 0HA, England.
[Sturm, E.] Max Planck Inst Extraterr Phys, D-85741 Garching, Germany.
RP Veilleux, S (reprint author), Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
EM veilleux@astro.umd.edu
OI Veilleux, Sylvain/0000-0002-3158-6820
FU NASA [GO2-13129X]; NASA Postdoctoral Program (NPP) Fellowship; Alexander
von Humboldt Foundation
FX We thank the anonymous referee for thoughtful and constructive comments
that improved this paper. Support for this work was provided by NASA
through Chandra contract GO2-13129X (S. V.) and the NASA Postdoctoral
Program (NPP) Fellowship (S. H. T., S. V.). S. V. acknowledges support
from the Alexander von Humboldt Foundation for a "renewed visit" to
Germany and thanks the host institution, MPE Garching, where a portion
of this paper was written. He is also grateful to R. Mushotzky for
discussions of the interpretation of the elemental abundances. This work
has made use of NASA's Astrophysics Data System Abstract Service and 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.
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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.
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PY 2014
VL 790
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SC Astronomy & Astrophysics
GA AL4PV
UT WOS:000339115800033
ER
PT J
AU Whitaker, KE
Rigby, JR
Brammer, GB
Gladders, MD
Sharon, K
Teng, SH
Wuyts, E
AF Whitaker, Katherine E.
Rigby, Jane R.
Brammer, Gabriel B.
Gladders, Michael D.
Sharon, Keren
Teng, Stacy H.
Wuyts, Eva
TI RESOLVED STAR FORMATION ON SUB-GALACTIC SCALES IN A MERGER AT z=1.7
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: interactions; galaxies: starburst; gravitational lensing:
strong
ID SIMILAR-TO 2; INITIAL MASS FUNCTION; H-II REGIONS; GRAVITATIONALLY
LENSED GALAXIES; INTEGRAL FIELD SPECTROSCOPY; SUPERMASSIVE BLACK-HOLES;
HUBBLE-SPACE-TELESCOPE; DIGITAL SKY SURVEY; LESS-THAN 1.5; FORMING
GALAXIES
AB We present a detailed analysis of Hubble Space Telescope (HST) Wide Field Camera 3 (WFC3) G141 grism spectroscopy for seven star-forming regions of the highly magnified lensed starburst galaxy RCSGA 032727-132609 at z = 1.704. We measure the spatial variations of the extinction in RCS0327 through the observed H gamma/H beta emission line ratios, finding a constant average extinction of E(B - V)(gas) = 0.40 +/- 0.07. We infer that the star formation is enhanced as a result of an ongoing interaction, with measured star formation rates derived from demagnified, extinction-corrected H beta line fluxes for the individual star-forming clumps falling >1-2 dex above the star formation sequence. When combining the HST/WFC3 [O III] lambda 5007/H beta emission line ratio measurements with [N II]/H alpha line ratios from Wuyts et al., we find that the majority of the individual star-forming regions fall along the local "normal" abundance sequence. With the first detections of the He I lambda 5876 and He II lambda 4686 recombination lines in a distant galaxy, we probe the massive-star content of the star-forming regions in RCS0327. The majority of the star-forming regions have a He I lambda 5876 to H beta ratio consistent with the saturated maximum value, which is only possible if they still contain hot O-stars. Two regions have lower ratios, implying that their last burst of new star formation ended similar to 5 Myr ago. Together, the He I lambda 5876 and He II lambda 4686 to H beta line ratios provide indirect evidence for the order in which star formation is stopping in individual star-forming knots of this high-redshift merger. We place the spatial variations of the extinction, star formation rate and ionization conditions in the context of the star formation history of RCS0327.
C1 [Whitaker, Katherine E.; Rigby, Jane R.; Teng, Stacy H.] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA.
[Brammer, Gabriel B.] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
[Gladders, Michael D.] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA.
[Gladders, Michael D.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA.
[Sharon, Keren] Univ Michigan, Dept Astron & Astrophys, Ann Arbor, MI 48109 USA.
[Wuyts, Eva] Max Planck Inst Extraterr Phys MPE, D-85748 Garching, Germany.
RP Whitaker, KE (reprint author), NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Code 665, Greenbelt, MD 20771 USA.
EM kate.whitaker@nasa.gov
RI Rigby, Jane/D-4588-2012;
OI Rigby, Jane/0000-0002-7627-6551; Brammer, Gabriel/0000-0003-2680-005X
FU NASA Postdoctoral Program at the Goddard Space Flight Center; NASA [NAS
5-26555, NAS5-26555]; NASA from the Space Telescope Science Institute
[12726]
FX The authors acknowledge Alaina Henry for insightful discussions, and
Alejo Stark for his help with the AGN analysis. We thank the anonymous
referee for useful comments and a careful reading of the paper. K.E.W.
is 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. This research is based on
observations made with the NASA/ESA Hubble Space Telescope, obtained at
the Space Telescope Science Institute, which is operated by the
Association of Universities for Research in Astronomy, Inc., under NASA
contract NAS 5-26555. These observations are associated with program
12726. Support for program number 12726 was provided by NASA through a
grant from the Space Telescope Science Institute, which is operated by
the Association of Universities for Research in Astronomy, Inc., under
NASA contract NAS5-26555. We thank Gary Ferland and Claus Leitherer for
making the Cloudy and Starbust99 tools publicly available.
NR 115
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SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD AUG 1
PY 2014
VL 790
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AR 143
DI 10.1088/0004-637X/790/2/143
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AL4PV
UT WOS:000339115800060
ER
PT J
AU Williams, BJ
Borkowski, KJ
Reynolds, SP
Ghavamian, P
Raymond, JC
Long, KS
Blair, WP
Sankrit, R
Winkler, PF
Hendrick, SP
AF Williams, Brian J.
Borkowski, Kazimierz J.
Reynolds, Stephen P.
Ghavamian, Parviz
Raymond, John C.
Long, Knox S.
Blair, William P.
Sankrit, Ravi
Winkler, P. Frank
Hendrick, Sean P.
TI SPITZER OBSERVATIONS OF THE TYPE IA SUPERNOVA REMNANT N103B: KEPLER'S
OLDER COUSIN?
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE dust, extinction; ISM: supernova remnants
ID LARGE-MAGELLANIC-CLOUD; RESOLUTION X-RAY; SN 1006; COSMIC SILICATES;
DUST; PROGENITOR; EMISSION; STARS; SHOCK; IDENTIFICATION
AB We report results from Spitzer observations of SNR 0509-68.7, also known as N103B, a young Type Ia supernova remnant (SNR) in the Large Magellanic Cloud (LMC) that shows interaction with a dense medium in its western hemisphere. Our images show that N103B has strong IR emission from warm dust in the post-shock environment. The post-shock gas density we derive, 45 cm(-3), is much higher than in other Type Ia remnants in the LMC, though a lack of spatial resolution may bias measurements toward regions of higher than average density. This density is similar to that in Kepler's SNR, a Type Ia interacting with a circumstellar medium (CSM). Optical images show Ha emission along the entire periphery of the western portion of the shock, with [O III] and [S II] lines emitted from a few dense clumps of material where the shock has become radiative. The dust is silicate in nature, though standard silicate dust models fail to reproduce the "18 mu m" silicate feature that peaks instead at 17.3 mu m. We propose that the dense material is circumstellar material lost from the progenitor system, as with Kepler. If the CSM interpretation is correct, this remnant would become the second member, along with Kepler, of a class of Type Ia remnants characterized by interaction with a dense CSM hundreds of years post-explosion. A lack of N enhancement eliminates symbiotic asymptotic giant branch progenitors. The white dwarf companion must have been relatively unevolved at the time of the explosion.
C1 [Williams, Brian J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Borkowski, Kazimierz J.; Reynolds, Stephen P.] N Carolina State Univ, Dept Phys, Raleigh, NC 27695 USA.
[Ghavamian, Parviz] Towson Univ, Dept Phys Chem & Geosci, Towson, MD 21252 USA.
[Raymond, John C.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Long, Knox S.] STScI, Baltimore, MD 21218 USA.
[Blair, William P.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA.
[Sankrit, Ravi] NASA, Ames Res Ctr, SOFIA Sci Ctr, Moffett Field, CA 94035 USA.
[Winkler, P. Frank] Middlebury Coll, Dept Phys, Middlebury, VT 05753 USA.
[Hendrick, Sean P.] Millersville Univ Pennsylvania, Dept Phys, Millersville, PA 17551 USA.
RP Williams, BJ (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
EM brian.j.williams@nasa.gov
FU Spitzer Guest Observer [RSA 1265236, RSA 1328682]
FX We thank R. Chris Smith for providing the optical images from CTIO. This
work was supported through Spitzer Guest Observer Grants RSA 1265236 and
RSA 1328682.
NR 54
TC 7
Z9 7
U1 0
U2 0
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 AUG 1
PY 2014
VL 790
IS 2
AR 139
DI 10.1088/0004-637X/790/2/139
PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AL4PV
UT WOS:000339115800056
ER
PT J
AU Suggs, RM
Moser, DE
Cooke, WJ
Suggs, RJ
AF Suggs, R. M.
Moser, D. E.
Cooke, W. J.
Suggs, R. J.
TI The flux of kilogram-sized meteoroids from lunar impact monitoring
SO ICARUS
LA English
DT Article
DE Meteors; Moon; Photometry; Near-Earth Objects; Cratering
ID CAMERA NETWORK; MOON; FLASHES; EARTH; STREAMS; SURFACE; SEARCH; STARS
AB The flashes from meteoroid impacts on the Moon are useful in determining the flux of impactors with masses as low as a few tens of grams. A routine monitoring program at NASA's Marshall Space Flight Center has recorded over 300 impacts since 2006. A selection of 126 flashes recorded during periods of photometric skies was analyzed, creating the largest and most homogeneous dataset of lunar impact flashes to date. Standard CCD photometric techniques were applied to the video and the luminous energy, kinetic energy, and mass are estimated for each impactor. Shower associations were determined for most of the impactors and a range of luminous efficiencies was considered. The flux to a limiting energy of 2.5 x 10(-6) kT TNT or 1.05 x 10(7) J is 1.03 x 10(-7) km(-2) h(-1) and the flux to a limiting mass of 30 g is 6.14 x 10(-1) m(-2) yr(-1) at the Moon. Comparisons made with measurements and models of the meteoroid population indicate that the flux of objects in this size range is slightly lower (but within the error bars) than flux at this size from the power law distribution determined for the near Earth object and fireball population by Brown et al. (Brown, P.G., Spalding, R., ReVelle, D., Tagliaferri, E., Worden, S. [2002]. Nature 420, 294-296). Size estimates for the crater detected by Lunar Reconnaissance Orbiter from a large impact observed on March 17, 2013 are also briefly discussed. Published by Elsevier Inc.
C1 [Suggs, R. M.; Cooke, W. J.; Suggs, R. J.] NASA, George C Marshall Space Flight Ctr, Meteoroid Environm Off, Nat Environm Branch, Huntsville, AL 35812 USA.
[Moser, D. E.] MITS Dynet, George C Marshall Space Flight Ctr, Meteoroid Environm Off, Nat Environm Branch, Huntsville, AL 35812 USA.
RP Suggs, RM (reprint author), NASA, George C Marshall Space Flight Ctr, Meteoroid Environm Off, Nat Environm Branch, EV44 Marshall Space Flight Ctr, Huntsville, AL 35812 USA.
EM rob.suggs@nasa.gov
FU NASA Meteoroid Environment Office, Marshall Space Flight Center
Engineering Directorate; International Space Station Program,
Constellation Program; Space Shuttle Program
FX The authors gratefully acknowledge the NASA Meteoroid Environment
Office, Marshall Space Flight Center Engineering Directorate, the
International Space Station Program, Constellation Program, and Space
Shuttle Program for financial support for this work. We appreciate the
dedication of the following personnel who operated the telescopes and
helped analyze the data: Richard Altstatt, Victoria Coffey, Anne
Diekmann, Heather Koehler, and Leigh Smith. We also thank Peter Gural
for providing the LunarScan software which was essential in performing
this work and Rhiannon Blaauw who developed the meteor shower catalog
for us. Thanks also to George Varros and Dave Clark for independent
confirmation of 3 of the flashes. We owe a huge debt of gratitude to
Wesley Swift who helped assemble the observatories and developed the
initial photometric analysis software as well as collecting and
analyzing some of the data.
NR 62
TC 16
Z9 16
U1 2
U2 6
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 AUG
PY 2014
VL 238
BP 23
EP 36
DI 10.1016/j.icarus.2014.04.032
PG 14
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AL8CV
UT WOS:000339366400003
ER
PT J
AU Burger, MH
Killen, RM
McClintock, WE
Merkel, AW
Vervack, RJ
Cassidy, TA
Sarantos, M
AF Burger, Matthew H.
Killen, Rosemary M.
McClintock, William E.
Merkel, Aimee W.
Vervack, Ronald J., Jr.
Cassidy, Timothy A.
Sarantos, Menelaos
TI Seasonal variations in Mercury's dayside calcium exosphere
SO ICARUS
LA English
DT Article
DE Mercury; Mercury, atmosphere; Spectroscopy; Atmospheres, structure
ID INPUT FUNCTION; SODIUM; ATMOSPHERE; IMPACTS; MODEL; FLUX
AB The Mercury Atmospheric and Surface Composition Spectrometer on the MESSENGER spacecraft has observed calcium emission in Mercury's exosphere on a near-daily basis since March 2011. During MESSENGER's primary and first extended missions (March 2011 - March 2013) the dayside calcium exosphere was measured over eight Mercury years. We have simulated these data with a Monte Carlo model of exospheric source processes to show that (a) there is a persistent source of energetic calcium located in the dawn equatorial region, (b) there is a seasonal dependence in the calcium source rate, and (c) there are no obvious year-to-year variations in the near-surface dayside calcium exosphere. (C) 2014 Elsevier Inc. All rights reserved.
C1 [Burger, Matthew H.] Morgan State Univ, Goddard Earth Sci Technol & Res, Baltimore, MD 21251 USA.
[Killen, Rosemary M.] NASA, Solar Syst Explorat Div, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[McClintock, William E.; Merkel, Aimee W.; Cassidy, Timothy A.] Univ Colorado, Atmospher & Space Phys Lab, Boulder, CO 80309 USA.
[Vervack, Ronald J., Jr.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA.
[Sarantos, Menelaos] Univ Maryland Baltimore Cty, Goddard Planetary Heliophys Inst, Baltimore, MD 21228 USA.
RP Burger, MH (reprint author), Morgan State Univ, Goddard Earth Sci Technol & Res, Baltimore, MD 21251 USA.
EM Matthew.Burger@nasa.gov
RI Vervack, Ronald/C-2702-2016
OI Vervack, Ronald/0000-0002-8227-9564
NR 27
TC 14
Z9 14
U1 2
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
EI 1090-2643
J9 ICARUS
JI Icarus
PD AUG
PY 2014
VL 238
BP 51
EP 58
DI 10.1016/j.icarus.2014.04.049
PG 8
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AL8CV
UT WOS:000339366400005
ER
PT J
AU Zimmerman, MI
Farrell, WM
Poppe, AR
AF Zimmerman, M. I.
Farrell, W. M.
Poppe, A. R.
TI Grid-free 2D plasma simulations of the complex interaction between the
solar wind and small, near-Earth asteroids
SO ICARUS
LA English
DT Article
DE Asteroids; Solar wind
ID LUNAR PHOTOELECTRON SHEATH; PONDED DEPOSITS; DUST; VACUUM; EXPANSION;
433-EROS; SPACE; MOON; WAKE
AB We present results from a new grid-free 2D plasma simulation code applied to a small, unmagnetized body immersed in the streaming solar wind plasma. The body was purposely modeled as an irregular shape in order to examine photoemission and solar wind plasma flow in high detail on the dayside, night-side, terminator and surface-depressed 'pocket' regions. Our objective is to examine the overall morphology of the various plasma interaction regions that form around a small body like a small near-Earth asteroid (NEA). We find that the object obstructs the solar wind flow and creates a trailing wake region downstream, which involves the interplay between surface charging and ambipolar plasma expansion. Photoemission is modeled as a steady outflow of electrons from illuminated portions of the surface, and under direct illumination the surface forms a non-monotonic or "double-sheath" electric potential upstream of the body, which is important for understanding trajectories and equilibria of lofted dust grains in the presence of a complex asteroid geometry. The largest electric fields are found at the terminators, where ambipolar plasma expansion in the body-sized nightside wake merges seamlessly with the thin photoelectric sheath on the dayside. The pocket regions are found to be especially complex, with nearby sunlit regions of positive potential electrically connected to unlit negative potentials and forming adjacent natural electric dipoles. For objects near the surface, we find electrical dissipation times (through collection of local environmental solar wind currents) that vary over at least 5 orders of magnitude: from 39 mu s inside the near-surface photoelectron cloud under direct sunlight to >> 1 s inside the particle-depleted nightside wake and shadowed pocket regions. (C) 2014 Elsevier Inc. All rights reserved.
C1 [Zimmerman, M. I.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA.
[Farrell, W. M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Poppe, A. R.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
[Zimmerman, M. I.; Farrell, W. M.; Poppe, A. R.] NASA, Lunar Sci Inst, Ames Res Ctr, Moffett Field, CA 94089 USA.
RP Zimmerman, MI (reprint author), Johns Hopkins Univ, Appl Phys Lab, 11100 Johns Hopkins Rd, Laurel, MD 20723 USA.
EM Michael.Zimmerman@jhuapl.edu
RI Farrell, William/I-4865-2013
FU NASA; NASA Lunar Science Institute; DREAM Virtual Institute [NNX09AG78A]
FX 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. Support by the
NASA Lunar Science Institute and DREAM Virtual Institute through Grant
NNX09AG78A are gratefully acknowledged. M. Zimmerman thanks W. Farrell
and T. Stubbs at NASA/GSFC for providing additional computing resources.
NR 41
TC 4
Z9 4
U1 0
U2 11
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 AUG
PY 2014
VL 238
BP 77
EP 85
DI 10.1016/j.icarus.2014.02.029
PG 9
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AL8CV
UT WOS:000339366400008
ER
PT J
AU Fletcher, LN
Greathouse, TK
Orton, GS
Irwin, PGJ
Mousis, O
Sinclair, JA
Giles, RS
AF Fletcher, Leigh N.
Greathouse, T. K.
Orton, G. S.
Irwin, P. G. J.
Mousis, O.
Sinclair, J. A.
Giles, R. S.
TI The origin of nitrogen on Jupiter and Saturn from the N-15/N-14 ratio
SO ICARUS
LA English
DT Article
DE Jupiter; Saturn; Atmospheres, composition
ID PROBE MASS-SPECTROMETER; GIANT PLANETS; CASSINI/CIRS OBSERVATIONS; CLOUD
STRUCTURE; SOLAR-SYSTEM; ISOTOPIC FRACTIONATION; JOVIAN ATMOSPHERE;
TITANS ATMOSPHERE; UPPER TROPOSPHERE; VOLATILES
AB The Texas Echelon cross Echelle Spectrograph (TEXES), mounted on NASA's Infrared Telescope Facility (IRTF), was used to map mid-infrared ammonia absorption features on both Jupiter and Saturn in February 2013. Ammonia is the principle reservoir of nitrogen on the giant planets, and the ratio of isotopologues (N-15/N-14) can reveal insights into the molecular carrier (e.g., as N-2 or NH3) of nitrogen to the forming protoplanets, and hence the source reservoirs from which these worlds accreted. We targeted two spectral intervals (900 and 960 cm(-1)) that were relatively clear of terrestrial atmospheric contamination and contained close features of (NH3)-N-14 and (NH3)-N-15, allowing us to derive the ratio from a single spectrum without ambiguity due to radiometric calibration (the primary source of uncertainty in this study). We present the first ground-based determination of Jupiter's N-15/N-14 ratio (in the range from 1.4 x 10(-3) to 2.5 x 10(-3)), which is consistent with both previous space-based studies and with the primordial value of the protosolar nebula. On Saturn, we present the first upper limit on the N-15/N-14 ratio of no larger than 2.0 x 10(-3) for the 900-cm(-1) channel and a less stringent requirement that the ratio be no larger than 2.8 x 10(-3) for the 960-cm(-1) channel (1 sigma-confidence). Specifically, the data rule out strong N-15-enrichments such as those observed in Titan's atmosphere and in cometary nitrogen compounds. To the extent possible with ground-based radiometric uncertainties, the saturnian and jovian N-15/N-14 ratios appear indistinguishable, implying that N-15-enriched ammonia ices could not have been a substantial contributor to the bulk nitrogen inventory of either planet. This result favours accretion of primordial N-2 on both planets, either in the gas phase from the solar nebula, or as ices formed at very low temperatures. Finally, spatially-resolved TEXES observations are used to derive zonal contrasts in tropospheric temperatures, phosphine and (NH3)-N-14 on both planets, allowing us to relate thermal conditions and chemical compositions to phenomena observed at visible wavelengths in 2013 (e.g., Jupiter's faint equatorial red colouration event and wave activity in the equatorial belts, plus the remnant warm band on Saturn following the 2010-11 springtime storm). (C) 2014 Elsevier Inc. All rights reserved.
C1 [Fletcher, Leigh N.; Irwin, P. G. J.; Sinclair, J. A.; Giles, R. S.] Univ Oxford, Clarendon Lab, Dept Phys, Oxford OX1 3PU, England.
[Greathouse, T. K.] SW Res Inst, Div 15, San Antonio, TX 78228 USA.
[Orton, G. S.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Mousis, O.] Univ Franche Comte, Inst UTINAM, CNRS INSU, UMR 6213, F-25030 Besancon, France.
RP Fletcher, LN (reprint author), Univ Oxford, Clarendon Lab, Dept Phys, Parks Rd, Oxford OX1 3PU, England.
EM fletcher@atm.ox.ac.uk
RI Fletcher, Leigh/D-6093-2011;
OI Fletcher, Leigh/0000-0001-5834-9588; Irwin, Patrick/0000-0002-6772-384X;
Giles, Rohini/0000-0002-7665-6562
FU Royal Society Research Fellowship at the University of Oxford; National
Aeronautics and Space Administration, Science Mission Directorate,
Planetary Astronomy Program [NNX-08AE38A]; Science and Technology
Facilities Council (STFC); CNES; NASA
FX Fletcher was supported by a Royal Society Research Fellowship at the
University of Oxford. Fletcher, Greathouse and Orton were visiting
astronomers at the Infrared Telescope Facility, which 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. The UK authors acknowledge the
support of the Science and Technology Facilities Council (STFC). Mousis
acknowledges support from CNES. A portion of this work was performed by
Orton at the Jet Propulsion Laboratory, California Institute of
Technology, under a contract with NASA. We are extremely grateful to
John Lacy and Matt Richter for their assistance in understanding the
performance of the TEXES instrument and the uncertainties related to
calibration, and to Tobias Owen for helpful discussions. We thank
Thierry Fouchet and one anonymous reviewer for their helpful critiques
of the manuscript.
NR 75
TC 10
Z9 10
U1 3
U2 6
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 AUG
PY 2014
VL 238
BP 170
EP 190
DI 10.1016/j.icarus.2014.05.007
PG 21
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AL8CV
UT WOS:000339366400015
ER
PT J
AU Altobelli, N
Lopez-Paz, D
Pilorz, S
Spilker, LJ
Morishima, R
Brooks, S
Leyrat, C
Deau, E
Edgington, S
Flandes, A
AF Altobelli, Nicolas
Lopez-Paz, David
Pilorz, S.
Spilker, Linda J.
Morishima, R.
Brooks, S.
Leyrat, C.
Deau, E.
Edgington, S.
Flandes, A.
TI Two numerical models designed to reproduce Saturn ring temperatures as
measured by Cassini-CIRS
SO ICARUS
LA English
DT Article
DE Saturn, rings; Planetary rings; Infrared observations
ID THERMAL INFRARED-EMISSION; DENSE PLANETARY RINGS; SELF-GRAVITY WAKES;
MAIN RINGS; MULTILAYER MODEL; SOLAR ELEVATION; VIMS; SIMULATIONS;
PARTICLES; DEPENDENCE
AB We present two numerical models designed to reproduce the temperatures of the illuminated Saturn rings as measured by the CASSINI-CIRS instrument. Our models are constrained by all available temperature measurements performed on the illuminated rings since SOI. Both models reproduce well the variations of temperature under any illumination and observation geometry. One model is derived from a purely numerical data mining approach, relying on the implementation of a Neural Network that treats the data set globally. This model is used as a test of coverage completeness of the observational parameter space, driving our ability to characterize the rings thermal response. The second (analytical) model is derived using simple physical considerations, by treating the rings as a surface rather than as a collection of individual particles, combined with an empirical anisotropy function to describe the temperature resulting from the Sun's and Saturn's heating. The thermal response of this ring-surface is parameterized by its Bond albedo and emissivity, thermal relaxation time and a set of geometrical parameters quantifying the anisotropy of the temperature measurements depending on azimuth and elevation of the observer with respect to the ring plane, as well as on the solar elevation. Both models provide formulae to predict the ring temperature, that will ease the benchmarking of future physical models against data. The physical model is applied to fit the temperature of tens of different radial slices, allowing us to constrain the combined emissivity and albedo, thermal relaxation time and anisotropy parameters of the ring slabs with the highest radial resolution achieved so far with CIRS. Using for the first time all observation geometries available for illuminated rings, we are confident that our values are as unbiased as possible against observation geometry. The thermal relaxation time appears to be short, a few tens of minutes, and independent of the radial distance across the whole ring. A study of the temperature anisotropy suggests inter-particle shadowing is important in the B ring and in the outer A ring regions. (C) 2014 Elsevier Inc. All rights reserved.
C1 [Altobelli, Nicolas; Lopez-Paz, David] ESA ESAC, Madrid, Spain.
[Pilorz, S.; Spilker, Linda J.; Morishima, R.; Brooks, S.; Deau, E.; Edgington, S.; Flandes, A.] NASA, Jet Prop Lab, Pasadena, CA 91109 USA.
[Leyrat, C.] Observ Paris, F-75014 Paris, France.
RP Altobelli, N (reprint author), ESA ESAC, Madrid, Spain.
EM nicolas.altobelli@sciops.esa.int
NR 33
TC 3
Z9 3
U1 1
U2 6
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 AUG
PY 2014
VL 238
BP 205
EP 220
DI 10.1016/j.icarus.2014.04.031
PG 16
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AL8CV
UT WOS:000339366400017
ER
PT J
AU Beck, J
Welch, T
Mitra, P
Reiff, K
Sun, XL
Abshire, J
AF Beck, Jeff
Welch, Terry
Mitra, Pradip
Reiff, Kirk
Sun, Xiaoli
Abshire, James
TI A Highly Sensitive Multi-element HgCdTe e-APD Detector for IPDA Lidar
Applications
SO JOURNAL OF ELECTRONIC MATERIALS
LA English
DT Article
DE HgCdTe; APD; NEP; IPDA; CO2; lidar
ID ELECTRON AVALANCHE PHOTODIODE
AB An HgCdTe electron avalanche photodiode (e-APD) detector has been developed for lidar receivers, one application of which is integrated path differential absorption lidar measurements of such atmospheric trace gases as CO2 and CH4. The HgCdTe APD has a wide, visible to mid-wave-infrared, spectral response, high dynamic range, substantially improved sensitivity, and an expected improvement in operational lifetime. A demonstration sensor-chip assembly consisting of a 4.3 mu m cutoff HgCdTe 4 x 4 APD detector array with 80 mu m pitch pixels and a custom complementary metal-oxide-semiconductor readout integrated circuit was developed. For one typical array the APD gain was 654 at 12 V with corresponding gain normalized dark currents ranging from 1.2 fA to 3.2 fA. The 4 x 4 detector system was characterized at 77 K with a 1.55 mu m wavelength, 1 mu s wide, laser pulse. The measured unit gain detector photon conversion efficiency was 91.1%. At 11 V bias the mean measured APD gain at 77 K was 307.8 with sigma/mean uniformity of 1.23%. The average, noise-bandwidth normalized, system noise-equivalent power (NEP) was 1.04 fW/Hz(1/2) with a sigma/mean of 3.8%. The measured, electronics-limited, bandwidth of 6.8 MHz was more than adequate for 1 mu s pulse detection. The system had an NEP (3 MHz) of 0.4 fW/Hz(1/2) at 12 V APD bias and a linear dynamic range close to 1000. A gain-independent quantum-limited SNR of 80% of full theoretical was indicative of a gain-independent excess noise factor very close to 1.0 and the expected APD mode quantum efficiency.
C1 [Beck, Jeff; Welch, Terry; Mitra, Pradip] DRS Technol Inc, Grp C4ISR, Dallas, TX 75243 USA.
[Reiff, Kirk] Analog Digital Integrated Circuits, Longwood, FL USA.
[Sun, Xiaoli; Abshire, James] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Beck, J (reprint author), DRS Technol Inc, Grp C4ISR, Dallas, TX 75243 USA.
EM jeff.beck@drs.com
FU NASA ESTO IIP-10 program
FX The authors would like to acknowledge the important contributions of DRS
employees James McCurdy (testing), Chris Kamilar (electronics), Mark
Skokan (fanout array design), Richard Scritchfield (consulting), Drew
Gordon (software), Patty Benken (array fabrication), and Towfik Teherani
(management support). This work was supported by the NASA ESTO IIP-10
program managed by Parminder Ghuman and Irene Bibyk.
NR 8
TC 5
Z9 5
U1 1
U2 22
PU SPRINGER
PI NEW YORK
PA 233 SPRING ST, NEW YORK, NY 10013 USA
SN 0361-5235
EI 1543-186X
J9 J ELECTRON MATER
JI J. Electron. Mater.
PD AUG
PY 2014
VL 43
IS 8
BP 2970
EP 2977
DI 10.1007/s11664-014-3164-8
PG 8
WC Engineering, Electrical & Electronic; Materials Science,
Multidisciplinary; Physics, Applied
SC Engineering; Materials Science; Physics
GA AL7SH
UT WOS:000339334800028
ER
PT J
AU Downs, ME
Hackney, KJ
Martin, D
Caine, TL
Cunningham, D
O'Connor, DP
Ploutz-Snyder, LL
AF Downs, Meghan E.
Hackney, Kyle J.
Martin, David
Caine, Timothy L.
Cunningham, David
O'Connor, Daniel P.
Ploutz-Snyder, Lori L.
TI Acute Vascular and Cardiovascular Responses to Blood Flow-Restricted
Exercise
SO MEDICINE AND SCIENCE IN SPORTS AND EXERCISE
LA English
DT Article
DE BLOOD FLOW-RESTRICTED EXERCISE; ARTERIAL BLOOD FLOW; CARDIOVASCULAR
RESPONSE TO RESISTANCE EXERCISE; HEMODYNAMIC RESPONSE TO RESISTANCE
EXERCISE
ID INTENSITY RESISTANCE EXERCISE; NEAR-INFRARED SPECTROSCOPY; MUSCLE
METABOREFLEX; NONINVASIVE MEASUREMENT; ARTERIAL STIFFNESS; DOPPLER
ULTRASOUND; INDOCYANINE GREEN; DYNAMIC EXERCISE; CARDIAC-OUTPUT; PRESSOR
REFLEX
AB Blood flow-restricted resistance exercise improves muscle strength; however, the cardiovascular response is not well understood. Purpose: This investigation measured local vascular responses, tissue oxygen saturation (StO(2)), and cardiovascular responses during supine unilateral leg press and heel raise exercise in four conditions: high load with no occlusion cuff, low load with no occlusion cuff, and low load with occlusion cuff pressure set at 1.3 times resting diastolic blood pressure (BFRDBP) or at 1.3 times resting systolic blood pressure (BFRSBP). Methods: Subjects (N = 13) (men/women, 5/8, 31.8 +/- 12.5 yr, 68.3 +/- 12.1 kg, mean +/- SD) performed three sets of leg press and heel raise to fatigue with 90-s rest. Artery diameter, velocity time integral, and stroke volume were measured using two-dimensional and Doppler ultrasound at rest and immediately after exercise. HR was monitored using a three-lead ECG. Finger blood pressure was acquired by photoplethysmography. Vastus lateralis StO(2) was measured using near-infrared spectroscopy. A repeated-measures ANOVA was used to analyze exercise work and StO(2). Multilevel modeling was used to evaluate the effect of exercise condition on vascular and cardiovascular variables. Statistical significance was set a priori at P < 0.05. Results: Artery diameter did not change from baseline during any of the exercise conditions. Blood flow increased after exercise in each condition except BFRSBP. StO(2) decreased during exercise and recovered to baseline levels during rest only in low load with no occlusion cuff and high load with no occlusion cuff. HR, stroke volume, and cardiac output (Q) over dot responses to exercise were blunted in blood flow-restricted exercise. Blood pressure was elevated during rest intervals in blood flow-restricted exercise. Conclusions: Our results demonstrate that cuff pressure alters the hemodynamic responses to resistance exercise. These findings warrant further evaluations in individuals presenting cardiovascular risk factors.
C1 [Downs, Meghan E.; O'Connor, Daniel P.] Univ Houston, Dept Hlth & Human Performance, Houston, TX USA.
[Hackney, Kyle J.; Martin, David; Caine, Timothy L.] Wyle Sci Technol & Engn Grp, Human Performance & Engn Div, Houston, TX USA.
[Hackney, Kyle J.] Syracuse Univ, Dept Exercise Sci, Syracuse, NY USA.
[Cunningham, David; Ploutz-Snyder, Lori L.] Univ Space Res Assoc, Houston, TX USA.
RP Ploutz-Snyder, LL (reprint author), NASA, Johnson Space Ctr, 2101 NASA Pkwy,B261,SK3, Houston, TX 77058 USA.
EM lori.ploutz-snyder-1@nasa.gov
FU National Aeronautics and Space Administration-Human Research Program
FX This study was funded by the National Aeronautics and Space
Administration-Human Research Program.
NR 45
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U1 6
U2 30
PU LIPPINCOTT WILLIAMS & WILKINS
PI PHILADELPHIA
PA 530 WALNUT ST, PHILADELPHIA, PA 19106-3621 USA
SN 0195-9131
EI 1530-0315
J9 MED SCI SPORT EXER
JI Med. Sci. Sports Exerc.
PD AUG
PY 2014
VL 46
IS 8
BP 1489
EP 1497
DI 10.1249/MSS.0000000000000253
PG 9
WC Sport Sciences
SC Sport Sciences
GA AL6RF
UT WOS:000339259700003
PM 24389514
ER
PT J
AU Saylor, RD
Wolfe, GM
Meyers, TP
Hicks, BB
AF Saylor, Rick D.
Wolfe, Glenn M.
Meyers, Tilden P.
Hicks, Bruce B.
TI A corrected formulation of the Multi layer Model (MLM) for inferring
gaseous dry deposition to vegetated surfaces
SO ATMOSPHERIC ENVIRONMENT
LA English
DT Article
DE Dry deposition; Nitric acid; Sulfur dioxide; Ozone; Multi-layer model;
Canopy; CASTNet
ID IONIZATION MASS-SPECTROMETER; CLEAN-AIR STATUS; TRENDS NETWORK; HNO3;
ATMOSPHERE; SULFUR
AB The Multilayer Model (MLM) has been used for many years to infer dry deposition fluxes from measured trace species concentrations and standard meteorological measurements for national networks in the U.S., including the U.S. Environmental Protection Agency's Clean Air Status and Trends Network (CASTNet). MLM utilizes a resistance analogy to calculate deposition velocities appropriate for whole vegetative canopies, while employing a multilayer integration to account for vertically varying meteorology, canopy morphology and radiative transfer within the canopy. However, the MLM formulation, as it was originally presented and as it has been subsequently employed, contains a non-physical representation related to the leaf-level quasi-laminar boundary layer resistance that affects the calculation of the total canopy resistance. In this note, the non-physical representation of the canopy resistance as originally formulated in MLM is discussed and a revised, physically consistent, formulation is suggested as a replacement. The revised canopy resistance formulation reduces estimates of HNO3 deposition velocities by as much as 38% during mid-day as compared to values generated by the original formulation. Inferred deposition velocities for SO2 and O-3 are not significantly altered by the change in formulation (<3%). Inferred deposition loadings of oxidized and total nitrogen from CASTNet data may be reduced by 10 20% and 5-10%, respectively, for the Eastern U. S. when employing the revised formulation of MLM as compared to the original formulation. Published by Elsevier Ltd. This is an open access article under the CC BY license (http://creativecommons.org/licenses/by/3.0/).
C1 [Saylor, Rick D.; Meyers, Tilden P.] NOAA, Air Resources Lab, Atmospher Turbulence & Diffus Div, Oak Ridge, TN 37830 USA.
[Wolfe, Glenn M.] NASA, Goddard Space Flight Ctr, Atmospher Chem & Dynam Lab, Greenbelt, MD 20771 USA.
[Wolfe, Glenn M.] Univ Maryland Baltimore Cty, Joint Ctr Earth Syst Technol, Baltimore, MD 21250 USA.
[Hicks, Bruce B.] Metcorps, Norris, TN 37828 USA.
RP Saylor, RD (reprint author), NOAA, Air Resources Lab, Atmospher Turbulence & Diffus Div, 456 S Illinois Ave, Oak Ridge, TN 37830 USA.
EM Rick.Saylor@noaa.gov
RI Wolfe, Glenn/D-5289-2011; Meyers, Tilden/C-6633-2016
FU U.S. Weather Research Program within the NOAA/OAR Office of Weather and
Air Quality
FX One author (RS) performed this work with support from the U.S. Weather
Research Program within the NOAA/OAR Office of Weather and Air Quality.
NR 21
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Z9 3
U1 2
U2 10
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 1352-2310
EI 1873-2844
J9 ATMOS ENVIRON
JI Atmos. Environ.
PD AUG
PY 2014
VL 92
BP 141
EP 145
DI 10.1016/j.atmosenv.2014.03.056
PG 5
WC Environmental Sciences; Meteorology & Atmospheric Sciences
SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences
GA AL0IO
UT WOS:000338810800015
ER
PT J
AU Lee, J
Kim, J
Lee, YG
AF Lee, Jaehwa
Kim, Jhoon
Lee, Yun Gon
TI Simultaneous retrieval of aerosol properties and clear-sky direct
radiative effect over the global ocean from MODIS
SO ATMOSPHERIC ENVIRONMENT
LA English
DT Article
DE Aerosol; Direct radiative effect; Radiative forcing; Ocean; MODIS
ID OPTICAL-PROPERTIES; ATMOSPHERE; CERES; TOP; INSTRUMENT; AERONET
AB A unified satellite algorithm is presented to simultaneously retrieve aerosol properties (aerosol optical depth; AOD and aerosol type) and clear-sky shortwave direct radiative effect (hereafter, DREA) over ocean. The algorithm is applied to Moderate Resolution Imaging spectroradiometer (MODIS) observations for a period from 2003 to 2010 to assess the DREA over the global ocean. The simultaneous retrieval utilizes lookup table (LUT) containing both spectral reflectances and solar irradiances calculated using a single radiative transfer model with the same aerosol input data. This study finds that aerosols cool the top-of-atmosphere (TOA) and bottom-of-atmosphere (BOA) by 5.2 +/- 0.5 W/m(2) and 8.3 W/m(2), respectively, and correspondingly warm the atmosphere (hereafter, ATM) by 3.1 W/m(2). These quantities, solely based on the MODIS observations, are consistent with those of previous studies incorporating chemical transport model simulations and satellite observations. However, the DREAs at BOA and ATM are expected to be less accurate compared to that of TOA due to low sensitivity in retrieving aerosol type information, which is related with the atmospheric heating by aerosols, particularly in low AOD conditions; consequently, the uncertainties could not be quantified. Despite the issue in the aerosol type information, the present method allows us to confine the DREA attributed only to fine-mode dominant aerosols, which are expected to be mostly anthropogenic origin, in the range from -1.1 W/m(2) to -1.3 W/m(2) at TOA. Improvements in size-resolved AOD and SSA retrievals from current and upcoming satellite instruments are suggested to better assess the DREA, particularly at BOA and ATM, where aerosol absorptivity induces substantial uncertainty. (C) 2014 Elsevier Ltd. All rights reserved.
C1 [Lee, Jaehwa; Kim, Jhoon; Lee, Yun Gon] Yonsei Univ, Inst Earth Astron & Atmosphere, Dept Atmospher Sci, Brain Korea Program 21, Seoul 120749, South Korea.
[Lee, Jaehwa] Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20742 USA.
[Lee, Jaehwa] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Lee, Yun Gon] Seoul Natl Univ, Sch Earth & Environm Sci, Seoul, South Korea.
RP Kim, J (reprint author), Yonsei Univ, Inst Earth Astron & Atmosphere, Dept Atmospher Sci, Brain Korea Program 21, Seoul 120749, South Korea.
EM jhoonkim1@gmail.com
OI Lee, Jaehwa/0000-0002-5029-476X
FU Korea Meteorological Administration Research and Development Program
[CATER 2012-2065]; Brain Korea 21 (BK21) program
FX We thank the MODIS science team for providing valuable data used in this
study. We also thank the principal investigators and their staff for
establishing and maintaining the AERONET sites used in this
investigation. This work was supported by the Korea Meteorological
Administration Research and Development Program under Grant CATER
2012-2065. This research was partially supported by the Brain Korea 21
(BK21) program for Jhoon Kim and Jaehwa Lee.
NR 25
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U1 1
U2 5
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 1352-2310
EI 1873-2844
J9 ATMOS ENVIRON
JI Atmos. Environ.
PD AUG
PY 2014
VL 92
BP 309
EP 317
DI 10.1016/j.atmosenv.2014.04.021
PG 9
WC Environmental Sciences; Meteorology & Atmospheric Sciences
SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences
GA AL0IO
UT WOS:000338810800033
ER
PT J
AU Flynn, CM
Pickering, KE
Crawford, JH
Lamsal, L
Krotkov, N
Herman, J
Weinheimer, A
Chen, G
Liu, X
Szykman, J
Tsay, SC
Loughner, C
Hains, J
Lee, P
Dickerson, RR
Stehr, JW
Brent, L
AF Flynn, Clare M.
Pickering, Kenneth E.
Crawford, James H.
Lamsal, Lok
Krotkov, Nickolay
Herman, Jay
Weinheimer, Andrew
Chen, Gao
Liu, Xiong
Szykman, James
Tsay, Si-Chee
Loughner, Christopher
Hains, Jennifer
Lee, Pius
Dickerson, Russell R.
Stehr, Jeffrey W.
Brent, Lacey
TI Relationship between column-density and surface mixing ratio:
Statistical analysis of O-3 and NO2 data from the July 2011 Maryland
DISCOVER-AQ mission
SO ATMOSPHERIC ENVIRONMENT
LA English
DT Article
DE Ozone; Nitrogen oxides; DISCOVER-AQ; Column-surface relationship;
Aircraft measurement campaign; Measurement-model comparison
ID TROPOSPHERIC OZONE; AIR-POLLUTANTS; UNITED-STATES; PART I; MODEL;
SATELLITE; POLLUTION; LAYER; OMI
AB To investigate the ability of column (or partial column) information to represent surface air quality, results of linear regression analyses between surface mixing ratio data and column abundances for O-3 and NO2 are presented for the July 2011 Maryland deployment of the DISCOVER-AQ mission. Data collected by the P-3B aircraft, ground-based Pandora spectrometers, Aura/OMI satellite instrument, and simulations for July 2011 from the CMAQ air quality model during this deployment provide a large and varied data set, allowing this problem to be approached from multiple perspectives. O-3 columns typically exhibited a statistically significant and high degree of correlation with surface data (R-2 > 0.64) in the P-3B data set, a moderate degree of correlation (0.16 < R-2 < 0.64) in the CMAQ data set, and a low degree of correlation (R-2 < 0.16) in the Pandora and OMI data sets. NO2 columns typically exhibited a low to moderate degree of correlation with surface data in each data set. The results of linear regression analyses for O-3 exhibited smaller errors relative to the observations than NO2 regressions. These results suggest that O-3 partial column observations from future satellite instruments with sufficient sensitivity to the lower troposphere can be meaningful for surface air quality analysis. (C) 2014 Elsevier Ltd. All rights reserved.
C1 [Flynn, Clare M.; Pickering, Kenneth E.; Dickerson, Russell R.; Stehr, Jeffrey W.; Brent, Lacey] Univ Maryland, Dept Atmospher & Ocean Sci, College Pk, MD 20742 USA.
[Pickering, Kenneth E.; Krotkov, Nickolay; Tsay, Si-Chee] NASA Goddard Space Flight Ctr, Greenbelt, MD USA.
[Crawford, James H.; Chen, Gao] NASA Langley Res Ctr, Hampton, VA USA.
[Lamsal, Lok] NASA Goddard Space Flight Ctr, GESTAR, Greenbelt, MD USA.
[Herman, Jay] NASA Goddard Space Flight Ctr, UMBC, Greenbelt, MD USA.
[Weinheimer, Andrew] NCAR Atmospher Chem Div, Boulder, CO USA.
[Liu, Xiong] Harvard Smithsonian Ctr Astrophys, Cambridge, MA USA.
[Szykman, James] EPA, Off Res & Dev, Washington, DC USA.
[Loughner, Christopher] NASA Goddard Space Flight Ctr, ESSIC, Greenbelt, MD USA.
[Hains, Jennifer] Maryland Dept Environm, Baltimore, MD 21224 USA.
[Lee, Pius] NOAA Air Resources Lab, Silver Spring, MD USA.
RP Flynn, CM (reprint author), Univ Maryland, Dept Atmospher & Ocean Sci, College Pk, MD 20742 USA.
EM cflynn@atmos.umd.edu
RI Liu, Xiong/P-7186-2014; Krotkov, Nickolay/E-1541-2012; Lee,
Pius/D-5201-2016; Pickering, Kenneth/E-6274-2012; Dickerson,
Russell/F-2857-2010;
OI Liu, Xiong/0000-0003-2939-574X; Krotkov, Nickolay/0000-0001-6170-6750;
Dickerson, Russell/0000-0003-0206-3083; Herman, Jay/0000-0002-9146-1632;
Loughner, Christopher/0000-0002-3833-2014
FU NASA Earth Venture-1 DISCOVER-AQ project [NNX10AR39G]
FX Funding for this work was provided by the NASA Earth Venture-1
DISCOVER-AQ project (NASA Grant NNX10AR39G). The authors thank Donald
Lenschow for providing estimates of PBL height during the deployment.
NR 34
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U1 4
U2 44
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 1352-2310
EI 1873-2844
J9 ATMOS ENVIRON
JI Atmos. Environ.
PD AUG
PY 2014
VL 92
BP 429
EP 441
DI 10.1016/j.atmosenv.2014.04.041
PG 13
WC Environmental Sciences; Meteorology & Atmospheric Sciences
SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences
GA AL0IO
UT WOS:000338810800045
ER
PT J
AU Dietrich, JP
Van Gaest, AL
Strickland, SA
Arkoosh, MR
AF Dietrich, Joseph P.
Van Gaest, Ahna L.
Strickland, Stacy A.
Arkoosh, Mary R.
TI The impact of temperature stress and pesticide exposure on mortality and
disease susceptibility of endangered Pacific salmon
SO CHEMOSPHERE
LA English
DT Article
DE Salmon; Malathion; Disease susceptibility; Temperature; Multiple
stressors
ID JUVENILE COHO SALMON; CHINOOK SALMON; CLIMATE-CHANGE; RIVER TEMPERATURE;
RISK-ASSESSMENT; TOXICITY; CONSERVATION; MIXTURES; INSECTICIDES;
ECOSYSTEMS
AB Anthropogenic stressors, including chemical contamination and temperature stress, may contribute to increased disease susceptibility in aquatic animals. Specifically, the organophosphate pesticide malathion has been detected in surface waters inhabited by threatened and endangered salmon. In the presence of increasing water temperatures, malathion may increase susceptibility to disease and ultimately threaten salmon survival. This work examines the effect of acute and sublethal exposures to malathion on ocean-type subyearling Chinook salmon held under two temperature regimes. Chinook salmon were exposed to malathion at optimal (11 degrees C) or elevated (19 and 20 degrees C) temperatures. The influence of temperature on the acute toxicity of malathion was determined by generating 96-h lethal concentration (LC) curves. A disease challenge assay was also used to assess the effects of sublethal malathion exposure. The malathion concentration that resulted in 50% mortality (LC50: 274.1 mu g L-1) of the Chinook salmon at 19 degrees C was significantly less than the LC50 at 11 degrees C (364.2 mu g L-1). Mortality increased 11.2% in Chinook salmon exposed to malathion at the elevated temperature and challenged with Aeromonas salmonicida compared to fish held at the optimal temperature and exposed to malathion or the carrier control. No difference in disease challenge mortality was observed among malathion-exposed and unexposed fish at the optimal temperature. The interaction of co-occurring stressors may have a greater impact on salmon than if they occur in isolation. Ecological risk assessments considering the effects of an individual stressor on threatened and endangered salmon may underestimate risk when additional stressors are present in the environment. Published by Elsevier Ltd.
C1 [Dietrich, Joseph P.; Van Gaest, Ahna L.; Strickland, Stacy A.; Arkoosh, Mary R.] NOAA, Environm & Fisheries Sci Div, NW Fisheries Sci Ctr, Natl Marine Fisheries Serv, Newport, OR 97365 USA.
RP Dietrich, JP (reprint author), NOAA, Environm & Fisheries Sci Div, NW Fisheries Sci Ctr, Natl Marine Fisheries Serv, 2032 SE OSU Dr, Newport, OR 97365 USA.
EM joseph.dietrich@noaa.gov; vangaest@gmail.com; sas70@me.com;
mary.arkoosh@noaa.gov
FU National Oceanic and Atmospheric Administration, Office of Protected
Resources
FX Funds were provided internally by the National Oceanic and Atmospheric
Administration, Office of Protected Resources. Individuals at the Office
of Protected Resources provided input into study design and objectives,
but did not participate in the collection, analysis, interpretation of
the data, preparation of the manuscript, or decision to submit the
manuscript. All experiments with the lab-raised salmon were in
accordance with the U.S. Government Principles for the Utilization and
Care of Vertebrate Animals Used in Testing. Research. and Training for
the humane treatment of fish to alleviate suffering.
NR 52
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U1 6
U2 63
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0045-6535
EI 1879-1298
J9 CHEMOSPHERE
JI Chemosphere
PD AUG
PY 2014
VL 108
BP 353
EP 359
DI 10.1016/j.chemosphere.2014.01.079
PG 7
WC Environmental Sciences
SC Environmental Sciences & Ecology
GA AJ7MU
UT WOS:000337881600046
PM 24559935
ER
PT J
AU Wan, ZM
Hong, Y
Khan, S
Gourley, J
Flamig, Z
Kirschbaum, D
Tang, GQ
AF Wan, Zhanming
Hong, Yang
Khan, Sadiq
Gourley, Jonathan
Flamig, Zachary
Kirschbaum, Dalia
Tang, Guoqiang
TI A cloud-based global flood disaster community cyber-infrastructure:
Development and demonstration
SO ENVIRONMENTAL MODELLING & SOFTWARE
LA English
DT Article
DE Flood; Cloud; Crowdsourcing; Web GIS
AB Flood disasters have significant impacts on the development of communities globally. This study describes a public cloud-based flood cyber-infrastructure (CyberFlood) that collects, organizes, visualizes, and manages several global flood databases for authorities and the public in real-time, providing location-based eventful visualization as well as statistical analysis and graphing capabilities. In order to expand and update the existing flood inventory, a crowdsourcing data collection methodology is employed for the public with smartphones or Internet to report new flood events, which is also intended to engage citizen-scientists so that they may become motivated and educated about the latest developments in satellite remote sensing and hydrologic modeling technologies. Our shared vision is to better serve the global water community with comprehensive flood information, aided by the state-of-the-art cloud computing and crowd-sourcing technology. The CyberFlood presents an opportunity to eventually modernize the existing paradigm used to collect, manage, analyze, and visualize water-related disasters. (C) 2014 Elsevier Ltd. All rights reserved.
C1 [Wan, Zhanming; Hong, Yang; Khan, Sadiq] Univ Oklahoma, Sch Civil Engn & Environm Sci, Norman, OK 73019 USA.
[Wan, Zhanming; Hong, Yang; Khan, Sadiq; Flamig, Zachary] Natl Weather Ctr, Hydrometeorol & Remote Sensing Lab HyDROS, Norman, OK 73072 USA.
[Wan, Zhanming; Hong, Yang; Khan, Sadiq; Flamig, Zachary] Natl Weather Ctr, Adv Radar Res Ctr, Norman, OK 73072 USA.
[Gourley, Jonathan; Flamig, Zachary] NOAA, Natl Severe Storms Lab, Natl Weather Ctr, Norman, OK 73069 USA.
[Kirschbaum, Dalia] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Tang, Guoqiang] Tsinghua Univ, Dept Hydraul Engn, Beijing 100084, Peoples R China.
RP Hong, Y (reprint author), Natl Weather Ctr, Adv Radar Res Ctr, HyDROS Lab, 4610 Suites,120 David L Boren Blvd, Norman, OK 73072 USA.
EM zwan@ou.edu; yanghong@ou.edu
RI Gourley, Jonathan/C-7929-2016; Hong, Yang/D-5132-2009;
OI Gourley, Jonathan/0000-0001-7363-3755; Hong, Yang/0000-0001-8720-242X;
Tang, Guoqiang/0000-0002-0923-583X
FU Hydrometeorology & Remote Sensing Lab (HyDROS); Advanced Radar Research
Center (ARRC) at the University of Oklahoma
FX The first author would like to acknowledge the seed money support from
Hydrometeorology & Remote Sensing Lab (HyDROS) and Advanced Radar
Research Center (ARRC) at the University of Oklahoma.
NR 15
TC 11
Z9 11
U1 4
U2 38
PU ELSEVIER SCI LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND
SN 1364-8152
EI 1873-6726
J9 ENVIRON MODELL SOFTW
JI Environ. Modell. Softw.
PD AUG
PY 2014
VL 58
BP 86
EP 94
DI 10.1016/j.envsoft.2014.04.007
PG 9
WC Computer Science, Interdisciplinary Applications; Engineering,
Environmental; Environmental Sciences
SC Computer Science; Engineering; Environmental Sciences & Ecology
GA AL0OI
UT WOS:000338825800007
ER
PT J
AU Ruzmaikin, A
Lee, JN
Wu, DL
AF Ruzmaikin, Alexander
Lee, Jae N.
Wu, Dong L.
TI Patterns of carbon monoxide in the middle atmosphere and effects of
solar variability
SO ADVANCES IN SPACE RESEARCH
LA English
DT Article
DE Middle atmosphere; Solar variability
ID CYCLE
AB We determine the spatial-time patterns of zonally averaged carbon monoxide (CO) in the middle atmosphere by applying Principle Component Analysis to the CO data obtained from the Microwave Limb Sounder (MLS) measurements on the Aura satellite in 2004-2012. The first two principal components characterize more than 90% of the CO variability. Both principal components are localized in the low thermosphere near the mesopause. The first principal component is asymmetric relative to the poles. It has opposite signs in the Northern and Southern Hemisphere at mid to high latitudes and strongly oscillates with an annual periodicity. The second principal component has the same sign in both hemispheres and oscillates mainly with a semi-annual frequency. Both principal components are modulated by the 11-year solar cycle and display short-term variations. To test possible correlations of these variations with the short term solar ultraviolet (UV) variability we use the simultaneous measurements of the UV solar radiance from the Solar-Stellar Irradiance Comparison Experiment (SOLSTICE) on the Solar Radiation and Climate Experiment (SORCE) satellite to investigate the correlation between CO in the middle atmosphere and solar UV in 2004-2012. Using a wavelet coherence technique a weak, intermittent 27-day signal is detected in high-frequency parts of the CO principal components. Published by Elsevier Ltd. on behalf of COSPAR.
C1 [Ruzmaikin, Alexander] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Lee, Jae N.] Univ Maryland Baltimore Cty, Joint Ctr Earth Syst Technol, Baltimore, MD 21250 USA.
[Wu, Dong L.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Ruzmaikin, A (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM Alexander.Ruzmaikin@jpl.nasa.gov
FU Jet Propulsion Laboratory of the California Institute of Technology
under the National Aeronautics and Space Administration; NASA LWS
FX We thank two reviewers for helpful critical comments. This work was
supported in part by the Jet Propulsion Laboratory of the California
Institute of Technology, under a contract with the National Aeronautics
and Space Administration. We acknowledge the NASA LWS grant on
observational study of solar variability impacts on the troposphere,
stratosphere and mesosphere.
NR 16
TC 4
Z9 4
U1 0
U2 6
PU ELSEVIER SCI LTD
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 AUG 1
PY 2014
VL 54
IS 3
BP 320
EP 326
DI 10.1016/j.asr.2013.06.033
PG 7
WC Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology &
Atmospheric Sciences
SC Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences
GA AL0IE
UT WOS:000338809800005
ER
PT J
AU Gao, J
Vissers, MR
Sandberg, M
Li, D
Cho, HM
Bockstiegel, C
Mazin, BA
Leduc, HG
Chaudhuri, S
Pappas, DP
Irwin, KD
AF Gao, J.
Vissers, M. R.
Sandberg, M.
Li, D.
Cho, H. M.
Bockstiegel, C.
Mazin, B. A.
Leduc, H. G.
Chaudhuri, S.
Pappas, D. P.
Irwin, K. D.
TI Properties of TiN for Detector and Amplifier Applications
SO JOURNAL OF LOW TEMPERATURE PHYSICS
LA English
DT Article
DE Kinetic inductance detector; Parametric amplifier; Two-level system;
Titanium nitride
ID BAND
AB We have experimentally explored and carefully characterized the important properties of TiN, including the resistivity, nonlinear kinetic inductance, the anomalous electro-dynamical response, and the two-level-system induced frequency shift and noise. We suggest that some of these properties, which are not well understood and are different from conventional superconductors, need further study and special consideration in kinetic inductance detector and parametric amplifier applications.
C1 [Gao, J.; Vissers, M. R.; Sandberg, M.; Li, D.; Cho, H. M.; Bockstiegel, C.; Pappas, D. P.; Irwin, K. D.] NIST, Boulder, CO 80305 USA.
[Mazin, B. A.] Univ Calif Santa Barbara, Santa Barbara, CA 93106 USA.
[Leduc, H. G.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Chaudhuri, S.] CALTECH, Pasadena, CA 91125 USA.
RP Gao, J (reprint author), NIST, Boulder, CO 80305 USA.
EM jgao@boulder.nist.gov
RI Mazin, Ben/B-8704-2011
OI Mazin, Ben/0000-0003-0526-1114
NR 20
TC 2
Z9 2
U1 1
U2 20
PU SPRINGER/PLENUM PUBLISHERS
PI NEW YORK
PA 233 SPRING ST, NEW YORK, NY 10013 USA
SN 0022-2291
EI 1573-7357
J9 J LOW TEMP PHYS
JI J. Low Temp. Phys.
PD AUG
PY 2014
VL 176
IS 3-4
BP 136
EP 141
DI 10.1007/s10909-014-1089-5
PG 6
WC Physics, Applied; Physics, Condensed Matter
SC Physics
GA AK1WY
UT WOS:000338210800002
ER
PT J
AU Giachero, A
Day, P
Falferi, P
Faverzani, M
Ferri, E
Giordano, C
Marghesin, B
Mattedi, F
Mezzena, R
Nizzolo, R
Nucciotti, A
AF Giachero, A.
Day, P.
Falferi, P.
Faverzani, M.
Ferri, E.
Giordano, C.
Marghesin, B.
Mattedi, F.
Mezzena, R.
Nizzolo, R.
Nucciotti, A.
TI Critical Temperature Tuning of Ti/TiN Multilayer Films Suitable for Low
Temperature Detectors
SO JOURNAL OF LOW TEMPERATURE PHYSICS
LA English
DT Article
DE MKIDs; Superconductive microresonator; Neutrino physics
AB We present our current progress on the design and test of Ti/TiN multilayer for use in kinetic inductance detectors. Sensors based on sub-stoichiometric TiN film are commonly used in several applications. However, it is difficult to control the targeted critical temperature , to maintain precise control of the nitrogen incorporation process and to obtain a production uniformity. To avoid these problems we investigated multilayer Ti/TiN films that show a high uniformity coupled with high quality factor, kinetic inductance and inertness of TiN. These features are ideal to realize superconductive microresonator detectors for astronomical instruments application but also for the field of neutrino physics. Using pure Ti and stoichiometric TiN, we developed and tested different multilayer configurations, in terms of number of Ti/TiN layers and in terms of different interlayer thicknesses. The target was to reach a critical temperature around K in order to have a low energy gap and slower recombination time (i.e. low generation-recombination noise). The results prove that the superconductive transition can be tuned in the K temperature range by properly choosing the Ti thickness in the nm range, and the TiN thickness in the nm range.
C1 [Giachero, A.; Faverzani, M.; Ferri, E.; Nizzolo, R.; Nucciotti, A.] Univ Milano Bicocca, Milan, Italy.
[Giachero, A.; Faverzani, M.; Ferri, E.; Nizzolo, R.; Nucciotti, A.] INFN Milano Bicocca, Milan, Italy.
[Day, P.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Falferi, P.] Fdn Bruno Kessler, CNR, Ist Foton & Nanotecnol, Trento, Italy.
[Giordano, C.; Marghesin, B.; Mattedi, F.] Fdn Bruno Kessler, Trento, Italy.
[Mezzena, R.] Univ Trento, Dipartimento Fis, Trento, Italy.
RP Giachero, A (reprint author), Univ Milano Bicocca, Milan, Italy.
EM Andrea.Giachero@mib.infn.it
RI Giachero, Andrea/I-1081-2013; Nucciotti, Angelo/I-8888-2012; Ferri,
Elena/L-8531-2014; Falferi, Paolo/C-3439-2015; Mezzena,
Renato/K-1802-2015; Faverzani, Marco/K-3865-2016
OI Giachero, Andrea/0000-0003-0493-695X; Nucciotti,
Angelo/0000-0002-8458-1556; Ferri, Elena/0000-0003-1425-3669; Falferi,
Paolo/0000-0002-1929-4710; Mezzena, Renato/0000-0001-9891-0472;
Faverzani, Marco/0000-0001-8119-2953
FU Fondazione Cariplo [2010-2351]
FX This work is supported by Fondazione Cariplo through the project
Development of Microresonator Detectors for Neutrino Physics (Grant
International Recruitment Call 2010, ref. 2010-2351).
NR 15
TC 1
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U1 0
U2 10
PU SPRINGER/PLENUM PUBLISHERS
PI NEW YORK
PA 233 SPRING ST, NEW YORK, NY 10013 USA
SN 0022-2291
EI 1573-7357
J9 J LOW TEMP PHYS
JI J. Low Temp. Phys.
PD AUG
PY 2014
VL 176
IS 3-4
BP 155
EP 160
DI 10.1007/s10909-013-1078-0
PG 6
WC Physics, Applied; Physics, Condensed Matter
SC Physics
GA AK1WY
UT WOS:000338210800005
ER
PT J
AU Kellaris, N
Daal, M
Epland, M
Pepin, M
Kamaev, O
Cushman, P
Kramer, E
Sadoulet, B
Mirabolfathi, N
Golwala, S
Runyan, M
AF Kellaris, N.
Daal, M.
Epland, M.
Pepin, M.
Kamaev, O.
Cushman, P.
Kramer, E.
Sadoulet, B.
Mirabolfathi, N.
Golwala, S.
Runyan, M.
TI Sub-Kelvin Thermal Conductivity and Radioactivity of Some Useful
Materials in Low Background Cryogenic Experiments
SO JOURNAL OF LOW TEMPERATURE PHYSICS
LA English
DT Article
DE Ti 15-3-3-3; Vespel; Graphite; Kapton; Thermal Conductivity;
Radioactivity
AB We present measurements of the thermal conductivity between 0.05 and 1 K, and radioactive contamination levels, for some thermally isolating materials. TIMET Ti 15-3-3-3, Mersen grade 2020 graphite, Vespel SP-1, Vespel SP-22, Vespel SCP-5000, Vespel SCP-5050, Graphlite CFRP, and a Kapton/epoxy composite are all investigated. Thermal conductivities were measured using a single-heater longitudinal heat flow method. Material radioactivity was determined for the materials at a low background counting facility using a high-purity gamma detector and GEANT4 Monte Carlo simulations.
C1 [Kellaris, N.; Daal, M.; Kramer, E.; Sadoulet, B.; Mirabolfathi, N.; Runyan, M.] Univ Calif Berkeley, Dept Phys, CDMS Expt, Berkeley, CA 94720 USA.
[Epland, M.; Pepin, M.; Cushman, P.] Univ Minnesota, Sch Phys & Astron, Minneapolis, MN 55455 USA.
[Kamaev, O.] Queens Univ, Dept Phys Engn Phys & Astron, Kingston, ON K7L 3N6, Canada.
[Golwala, S.] CALTECH, Div Phys Math & Astron, Pasadena, CA 91125 USA.
[Runyan, M.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Kellaris, N (reprint author), Univ Calif Berkeley, Dept Phys, CDMS Expt, Berkeley, CA 94720 USA.
EM nicholaskellaris@berkeley.edu
FU Department of Energy; National Science Foundation
FX The authors would like to thank Curbell Plastics and Tech-Etch for
donating test samples. This work was funded by the Department of Energy
and the National Science Foundation.
NR 9
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U1 2
U2 5
PU SPRINGER/PLENUM PUBLISHERS
PI NEW YORK
PA 233 SPRING ST, NEW YORK, NY 10013 USA
SN 0022-2291
EI 1573-7357
J9 J LOW TEMP PHYS
JI J. Low Temp. Phys.
PD AUG
PY 2014
VL 176
IS 3-4
BP 201
EP 208
DI 10.1007/s10909-013-1048-6
PG 8
WC Physics, Applied; Physics, Condensed Matter
SC Physics
GA AK1WY
UT WOS:000338210800012
ER
PT J
AU Karasik, BS
McKitterick, CB
Prober, DE
AF Karasik, Boris S.
McKitterick, Christopher B.
Prober, Daniel E.
TI Prospective Performance of Graphene HEB for Ultrasensitive Detection of
Sub-mm Radiation
SO JOURNAL OF LOW TEMPERATURE PHYSICS
LA English
DT Article
DE Graphene; Hot-electron bolometer; Noise thermometry
ID HOT-ELECTRON BOLOMETER; NOISE; NANOBOLOMETERS; MIXER; BAND
AB Noise equivalent power and time constant of a submillimeter wave hot-electron bolometer (HEB) made from monolayer graphene are analyzed using the lowest electron-phonon thermal conductance data reported to date. Frequency-domain multiplexed Johnson Noise Thermometry (JNT) is used for the detector readout. Planar microantennas or waveguides can provide efficient coupling of the graphene microdevice to radiation. The results show that the graphene HEB detector can be radiation background limited at very low level corresponding to the photon noise on a space telescope with cryogenically cooled mirror. Beside the high sensitivity, absence of a hard power saturation limit, higher operating temperature, and the ability to read 1,000s of elements with a single broadband amplifier will be the advantages of such a detector.
C1 [Karasik, Boris S.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[McKitterick, Christopher B.; Prober, Daniel E.] Yale Univ, Dept Phys, New Haven, CT 06520 USA.
[McKitterick, Christopher B.; Prober, Daniel E.] Yale Univ, Dept Appl Phys, New Haven, CT 06520 USA.
RP Karasik, BS (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM boris.s.karasik@jpl.nasa.gov
FU National Aeronautics and Space Administration; NSF [DMR-0907082]; IBM;
Yale University
FX The work at the Jet Propulsion Laboratory, California Institute of
Technology, was carried out under a contract with the National
Aeronautics and Space Administration. The work at Yale was supported by
NSF Grant DMR-0907082, an IBM Faculty Grant, and by Yale University.
NR 28
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PU SPRINGER/PLENUM PUBLISHERS
PI NEW YORK
PA 233 SPRING ST, NEW YORK, NY 10013 USA
SN 0022-2291
EI 1573-7357
J9 J LOW TEMP PHYS
JI J. Low Temp. Phys.
PD AUG
PY 2014
VL 176
IS 3-4
BP 249
EP 254
DI 10.1007/s10909-014-1087-7
PG 6
WC Physics, Applied; Physics, Condensed Matter
SC Physics
GA AK1WY
UT WOS:000338210800019
ER
PT J
AU McKitterick, C
Vora, H
Du, X
Karasik, B
Prober, D
AF McKitterick, Christopher B.
Vora, Heli
Du, Xu
Karasik, Boris S.
Prober, Daniel E.
TI Graphene Microbolometers with Superconducting Contacts for Terahertz
Photon Detection
SO JOURNAL OF LOW TEMPERATURE PHYSICS
LA English
DT Article
DE Graphene; Hot-electron bolometer; Terahertz
AB We report on noise and thermal conductance measurements taken in order to determine an upper bound on the performance of graphene as a terahertz photon detector. The main mechanism for sensitive terahertz detection in graphene is bolometric heating of the electron system. To study the properties of a device using this mechanism to detect terahertz photons, we perform Johnson noise thermometry measurements on graphene samples. These measurements probe the electron-phonon behavior of graphene on silicon dioxide at low temperatures. Because the electron-phonon coupling is weak in graphene, superconducting contacts with large gap are used to confine the hot electrons and prevent their out-diffusion. We use niobium nitride leads with a K to contact the graphene. We find these leads make good ohmic contact with very low contact resistance. Our measurements find an electron-phonon thermal conductance that depends quadratically on temperature above 4 K and is compatible with single terahertz photon detection.
C1 [McKitterick, Christopher B.; Prober, Daniel E.] Yale Univ, Dept Phys, New Haven, CT 06520 USA.
[McKitterick, Christopher B.; Prober, Daniel E.] Yale Univ, Dept Appl Phys, New Haven, CT 06520 USA.
[Vora, Heli; Du, Xu] SUNY Stony Brook, Dept Phys, Stony Brook, NY 11790 USA.
[Karasik, Boris S.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP McKitterick, CB (reprint author), Yale Univ, Dept Phys, New Haven, CT 06520 USA.
EM chris.mckitterick@yale.edu; daniel.prober@yale.edu
FU NSF [DMR-0907082]; IBM; Yale University; National Aeronautics and Space
Administration; AFOSR-YIP Award [FA9550-10-1-0090]
FX The work at Yale was supported by NSF Grant DMR-0907082, an IBM Faculty
Grant, and by Yale University. The work at Jet Propulson Laboratory was
carried out under a contract with the National Aeronautics and Space
Administration. X. Du and H. Vora acknowledge support from AFOSR-YIP
Award No. FA9550-10-1-0090.
NR 26
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U2 39
PU SPRINGER/PLENUM PUBLISHERS
PI NEW YORK
PA 233 SPRING ST, NEW YORK, NY 10013 USA
SN 0022-2291
EI 1573-7357
J9 J LOW TEMP PHYS
JI J. Low Temp. Phys.
PD AUG
PY 2014
VL 176
IS 3-4
BP 291
EP 298
DI 10.1007/s10909-014-1127-3
PG 8
WC Physics, Applied; Physics, Condensed Matter
SC Physics
GA AK1WY
UT WOS:000338210800026
ER
PT J
AU Beyer, AD
Kenyon, ME
Bumble, B
Runyan, MC
Echternach, PE
Holmes, WA
Bock, JJ
Bradford, CM
AF Beyer, A. D.
Kenyon, M. E.
Bumble, B.
Runyan, M. C.
Echternach, P. E.
Holmes, W. A.
Bock, J. J.
Bradford, C. M.
TI Comparing Transition-Edge Sensor Response Times in a Modified Contact
Scheme with Different Support Beams
SO JOURNAL OF LOW TEMPERATURE PHYSICS
LA English
DT Article
DE Infrared detector; Sub-mm detector; Superconducting device;
Transition-edge sensor
AB We present measurements of the thermal conductance, G, and effective time constants, , of three transition-edge sensors (TESs) populated in arrays operated from 80-87 mK with T 120 mK. Our TES arrays include several variations of thermal architecture enabling determination of the architecture that demonstrates the minimum noise equivalent power, the lowest , and the trade-offs among designs. The three TESs we report here have identical Mo/Cu bilayer thermistors and wiring structures, while the thermal architectures are: (1) a TES with straight support beams of 1 mm length, (2) a TES with meander support beams of total length 2 mm and with two phonon-filter blocks per beam, and (3) a TES with meander support beams of total length 2 mm and with six phonon-filter blocks per beam. Our wiring scheme aims to lower the thermistor normal state resistance R and increase the sharpness of the transition dlogR/dlogT at the transition temperature T. We find an upper limit of given by (), and G values of 200 fW/K for (1), 15 fW/K for (2), and 10 fW/K for (3). The value of can be improved by slightly increasing the length of our thermistors.
C1 [Beyer, A. D.; Kenyon, M. E.; Bumble, B.; Runyan, M. C.; Echternach, P. E.; Holmes, W. A.; Bock, J. J.; Bradford, C. M.] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
RP Beyer, AD (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91125 USA.
EM andrew.d.beyer@jpl.nasa.gov
NR 7
TC 0
Z9 0
U1 1
U2 3
PU SPRINGER/PLENUM PUBLISHERS
PI NEW YORK
PA 233 SPRING ST, NEW YORK, NY 10013 USA
SN 0022-2291
EI 1573-7357
J9 J LOW TEMP PHYS
JI J. Low Temp. Phys.
PD AUG
PY 2014
VL 176
IS 3-4
BP 299
EP 303
DI 10.1007/s10909-013-1027-y
PG 5
WC Physics, Applied; Physics, Condensed Matter
SC Physics
GA AK1WY
UT WOS:000338210800027
ER
PT J
AU Morgan, KM
Busch, SE
Eckart, ME
Kilbourne, CA
McCammon, D
AF Morgan, K. M.
Busch, S. E.
Eckart, M. E.
Kilbourne, C. A.
McCammon, D.
TI Large Area Transition Edge Sensor X-ray Microcalorimeters for Diffuse
X-ray Background Studies
SO JOURNAL OF LOW TEMPERATURE PHYSICS
LA English
DT Article
DE Transition edge sensors; Microcalorimeters; X-ray astronomy
ID CHARGE-TRANSFER; SOLAR-WIND; EMISSION
AB We are developing transition edge sensor (TES) mirocalorimeters with large area (0.72 mm) absorbers to study the keV diffuse X-ray background. The goal is to develop a 2 cm array of 256 pixels for a sounding rocket payload. We present a pixel design which includes a Mo/Au bilayer TES coupled to a large (850 x 850 x 0.2 m) gold absorber. Our simulations indicate that such a design can achieve energy resolution as good as 1.6 eV FWHM in our target bandpass of 0.05-1 keV. Additionally, thermal modelling shows that for typical gold layers, the position-dependent variation of the pulse shape over the large area of the absorber is not expected to significantly degrade this energy resolution. An array of devices will be fabricated in late 2013 to test this design.
C1 [Morgan, K. M.; McCammon, D.] Univ Wisconsin, Dept Phys, Madison, WI 53706 USA.
[Busch, S. E.; Eckart, M. E.; Kilbourne, C. A.] NASA, Goddard Space Flight Ctr, Xray Astrophys Lab, Greenbelt, MD 20771 USA.
[Busch, S. E.] NASA, Postdoctoral Program, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Eckart, M. E.] CRESST, Baltimore, MD 21250 USA.
[Eckart, M. E.] Univ Maryland Baltimore Cty, Baltimore, MD 21250 USA.
RP Morgan, KM (reprint author), Univ Wisconsin, Dept Phys, 1150 Univ Ave, Madison, WI 53706 USA.
EM kmmorgan2@wisc.edu
RI Morgan, Kelsey/J-5053-2016
OI Morgan, Kelsey/0000-0002-6597-1030
FU NASA Office of the Chief Technologist's Space Technology Research
Fellowship; NASA [NNX09AF09G]; NASA
FX This work was supported by a NASA Office of the Chief Technologist's
Space Technology Research Fellowship. Supported in part by NASA grant
NNX09AF09G. This research was in part supported by appointment (S. E.
Busch) to the NASA Postdoctoral Program at Goddard Space Flight Center,
administered by Oak Ridge Associated Universities through a contract
with NASA.
NR 14
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U1 1
U2 13
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PI NEW YORK
PA 233 SPRING ST, NEW YORK, NY 10013 USA
SN 0022-2291
EI 1573-7357
J9 J LOW TEMP PHYS
JI J. Low Temp. Phys.
PD AUG
PY 2014
VL 176
IS 3-4
BP 331
EP 336
DI 10.1007/s10909-013-1011-6
PG 6
WC Physics, Applied; Physics, Condensed Matter
SC Physics
GA AK1WY
UT WOS:000338210800032
ER
PT J
AU Smith, SJ
Adams, JS
Bandler, SR
Busch, SE
Chervenak, JA
Eckart, ME
Finkbeiner, FM
Kelley, RL
Kilbourne, CA
Lee, SJ
Porst, JP
Porter, FS
Sadleir, JE
AF Smith, S. J.
Adams, J. S.
Bandler, S. R.
Busch, S. E.
Chervenak, J. A.
Eckart, M. E.
Finkbeiner, F. M.
Kelley, R. L.
Kilbourne, C. A.
Lee, S. J.
Porst, J. -P.
Porter, F. S.
Sadleir, J. E.
TI Characterization of Mo/Au Transition-Edge Sensors with Different
Geometric Configurations
SO JOURNAL OF LOW TEMPERATURE PHYSICS
LA English
DT Article
DE Transition-edge sensor; Microcalorimeter; Weak-link; Proximity effect
ID X-RAY MICROCALORIMETERS
AB Mo/Au transition-edge sensors exhibit weak-link behavior in the measured temperature, and field, dependence of the critical current . This is a consequence of the longitudinal proximitization between the Nb electrical bias contacts and the bilayer. Understanding how weak-link superconductivity impacts the resistive transition and the detector energy resolution is of great interest. In this contribution we present studies of for three devices that have different geometries of metallic depositions on top of the sensor used for noise mitigation and X-ray absorption. Results show that these features change the measured compared to the previously seen measurements on devices without additional deposition layers. Measurements of the small signal transition parameters and also reveal differences between designs that impact the measured response to X-rays and energy resolution.
C1 [Smith, S. J.; Adams, J. S.; Bandler, S. R.; Busch, S. E.; Chervenak, J. A.; Eckart, M. E.; Finkbeiner, F. M.; Kelley, R. L.; Kilbourne, C. A.; Lee, S. J.; Porst, J. -P.; Porter, F. S.; Sadleir, J. E.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Smith, S. J.; Adams, J. S.; Eckart, M. E.] CRESST, Baltimore, MD 21250 USA.
[Smith, S. J.; Adams, J. S.; Eckart, M. E.] Univ Maryland Baltimore Cty, Baltimore, MD 21250 USA.
[Bandler, S. R.] CRESST, College Pk, MD 20742 USA.
[Bandler, S. R.] Univ Maryland, College Pk, MD 20742 USA.
[Busch, S. E.; Lee, S. J.] NASA, Postdoctoral Program Fellow, Greenbelt, MD USA.
[Finkbeiner, F. M.] Wyle Informat Syst, Mclean, VA 22102 USA.
[Porst, J. -P.] CRESST, Columbia, MD 21044 USA.
[Porst, J. -P.] USRA, Columbia, MD 21044 USA.
RP Smith, SJ (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
EM stephen.j.smith@nasa.gov
RI Smith, Stephen/B-1256-2008; Bandler, Simon/A-6258-2010; Lee, Sang
Jun/A-3892-2015; Porter, Frederick/D-3501-2012
OI Smith, Stephen/0000-0003-4096-4675; Bandler, Simon/0000-0002-5112-8106;
Lee, Sang Jun/0000-0002-8199-3993; Porter, Frederick/0000-0002-6374-1119
FU NASA
FX This research was in part supported by an appointment (Busch and Lee) to
the NASA Postdoctoral Program at Goddard Space Flight Center,
administered by Oak Ridge Associated Universities through a contract
with NASA.
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U2 19
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PI NEW YORK
PA 233 SPRING ST, NEW YORK, NY 10013 USA
SN 0022-2291
EI 1573-7357
J9 J LOW TEMP PHYS
JI J. Low Temp. Phys.
PD AUG
PY 2014
VL 176
IS 3-4
BP 356
EP 362
DI 10.1007/s10909-013-1031-2
PG 7
WC Physics, Applied; Physics, Condensed Matter
SC Physics
GA AK1WY
UT WOS:000338210800036
ER
PT J
AU Kenyon, M
Beyer, AD
Bumble, B
Echternach, PM
Holmes, WA
Bradford, CM
AF Kenyon, M.
Beyer, A. D.
Bumble, B.
Echternach, P. M.
Holmes, W. A.
Bradford, C. M.
TI Toward a Detector/Readout Architecture for the Background-Limited
Far-IR/Submm Spectrograph (BLISS)
SO JOURNAL OF LOW TEMPERATURE PHYSICS
LA English
DT Article
DE Transition-edge sensor; Far-IR spectrometer; Submm spectrometer
AB We have built and tested 32-element linear arrays of absorber-coupled transition-edge sensors (TESs) read out with a time-division SQUID multiplexer. This detector/readout architecture is designed for the background-limited far-IR/submm spectrograph (BLISS) which is a broadband (35-433 m), grating spectrometer consisting of six wavebands each with a modest resolution of R 700. Since BLISS requires the effective noise equivalent power (NEP) of the TESs to equal 1 10 W/Hz, our detectors consist of very long (1-2 mm), narrow (0.4 m), and thin (0.25 m) SiN support beams that reduce the thermal conductance G between the substrate and the optical absorber. The thermistors of our lowest noise TESs consist of iridium with mK. We have measured the electrical properties of arrays of these Ir TESs with various meander and straight support beams and absorber shapes and found that G is 30 fW/K (meander) and 110 fW/K (straight), the electrical NEP is 2-3 10 W/Hz (meander and straight), and the response time is 10-30 ms (meander) and 2-5 ms (straight). To reduce spurious or "dark" power from heating the arrays, we mounted the arrays into light-tight niobium boxes and added custom L/R and L/C low-pass chip filters into these boxes to intercept dark power from the bias and readout circuit. We found the average dark power equals 1.3 and 4.6 fW for the boxes with L/R and L/C chip filters, respectively. We have built arrays with mK using molybdenum/copper bilayers and are working to lower the dark power by an order of magnitude so we can demonstrate NEP 10 W/Hz with these arrays. PACS numbers: 85.25.Pb; 95.85.Gn; 95.85.Fm; 63.22.+m.
C1 [Kenyon, M.; Beyer, A. D.; Bumble, B.; Echternach, P. M.; Holmes, W. A.; Bradford, C. M.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Kenyon, M (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM mkenyon@jpl.nasa.gov
FU National Aeronautics and Space Administration
FX This research was carried out at the Jet Propulsion Laboratory and
Caltech under contract with the National Aeronautics and Space
Administration.
NR 9
TC 0
Z9 0
U1 0
U2 3
PU SPRINGER/PLENUM PUBLISHERS
PI NEW YORK
PA 233 SPRING ST, NEW YORK, NY 10013 USA
SN 0022-2291
EI 1573-7357
J9 J LOW TEMP PHYS
JI J. Low Temp. Phys.
PD AUG
PY 2014
VL 176
IS 3-4
BP 376
EP 382
DI 10.1007/s10909-013-1020-5
PG 7
WC Physics, Applied; Physics, Condensed Matter
SC Physics
GA AK1WY
UT WOS:000338210800039
ER
PT J
AU Sadleir, JE
Lee, SJ
Smith, SJ
Busch, SE
Bandler, SR
Adams, JS
Eckart, ME
Chervenak, JA
Kelley, RL
Kilbourne, CA
Porter, FS
Porst, JP
AF Sadleir, John E.
Lee, Sang-Jun
Smith, Stephen J.
Busch, Sarah E.
Bandler, Simon R.
Adams, Joseph S.
Eckart, Megan E.
Chervenak, James A.
Kelley, Richard L.
Kilbourne, Caroline A.
Porter, Frederick S.
Porst, Jan-Patrick
TI The Magnetically-Tuned Transition-Edge Sensor
SO JOURNAL OF LOW TEMPERATURE PHYSICS
LA English
DT Article
DE Low temperature detectors; Supeconductivity; Magnetic field dependence;
Superconducting resistive transition width; Superconducting weak-links
AB We present the first measurements on the proposed magnetically-tuned superconducting transition-edge sensor and compare the modified resistive transition with the theoretical prediction (Sadleir et al., IEEE Trans App Supercond 23:2101405, 2013). A TES's resistive transition is customarily characterized in terms of the unitless device parameters and corresponding to the resistive response to changes in temperature and current respectively. We present a new relationship between measured IV quantities (sensor current and voltage ) and the parameters and and use these relations to confirm we have stably biased a TES with negative parameter with magnetic tuning. Motivated by access to this new unexplored parameter space, we investigate the conditions for bias stability of a TES taking into account both self and externally applied magnetic fields.
C1 [Sadleir, John E.; Lee, Sang-Jun; Smith, Stephen J.; Busch, Sarah E.; Bandler, Simon R.; Adams, Joseph S.; Eckart, Megan E.; Chervenak, James A.; Kelley, Richard L.; Kilbourne, Caroline A.; Porter, Frederick S.; Porst, Jan-Patrick] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Sadleir, JE (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
EM john.e.sadleir@nasa.gov
RI Smith, Stephen/B-1256-2008; Bandler, Simon/A-6258-2010; Lee, Sang
Jun/A-3892-2015; Porter, Frederick/D-3501-2012
OI Smith, Stephen/0000-0003-4096-4675; Bandler, Simon/0000-0002-5112-8106;
Lee, Sang Jun/0000-0002-8199-3993; Porter, Frederick/0000-0002-6374-1119
NR 7
TC 0
Z9 0
U1 2
U2 13
PU SPRINGER/PLENUM PUBLISHERS
PI NEW YORK
PA 233 SPRING ST, NEW YORK, NY 10013 USA
SN 0022-2291
EI 1573-7357
J9 J LOW TEMP PHYS
JI J. Low Temp. Phys.
PD AUG
PY 2014
VL 176
IS 3-4
BP 392
EP 399
DI 10.1007/s10909-014-1194-5
PG 8
WC Physics, Applied; Physics, Condensed Matter
SC Physics
GA AK1WY
UT WOS:000338210800041
ER
PT J
AU Lindeman, MA
Eom, BH
Day, PK
Swenson, LJ
Wernis, R
LeDuc, HG
Zmuidzinas, J
AF Lindeman, M. A.
Eom, B. H.
Day, P. K.
Swenson, L. J.
Wernis, Rebecca
LeDuc, H. G.
Zmuidzinas, J.
TI AC Bolometer Theory and Measurements of Kinetic Inductance
Bolometer-Resonators
SO JOURNAL OF LOW TEMPERATURE PHYSICS
LA English
DT Article
DE Alternating current; Bolometer; Calorimeter; Kinetic inductance; Theory;
Alpha; Beta; Response; Noise
AB AC bolometer theory is built on the established matrix formalism for quantum calorimeters and bolometers. The bolometer is represented by a 3 3 matrix with complex valued parameters. The bolometer matrix is used to model the behavior of the devices including the response to signal and noise, feedback, pulse response times, stability, and bolometer impedance. The effects of a current dependent bolometer impedance are included. The matrix simplifies theoretical computations of AC devices, including demodulation and the interactions between signals at different frequencies. This theory is applied to measurements of bolometers, each consisting of a kinetic inductance device suspended on a silicon nitride membrane. These measurements and analysis facilitate the optimization of the design and performance of these novel AC bolometers.
C1 [Lindeman, M. A.; Eom, B. H.; Day, P. K.; LeDuc, H. G.; Zmuidzinas, J.] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
[Swenson, L. J.; Wernis, Rebecca; Zmuidzinas, J.] CALTECH, Pasadena, CA 91125 USA.
RP Lindeman, MA (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91125 USA.
EM mark.a.lindeman@jpl.nasa.gov
NR 9
TC 3
Z9 3
U1 0
U2 6
PU SPRINGER/PLENUM PUBLISHERS
PI NEW YORK
PA 233 SPRING ST, NEW YORK, NY 10013 USA
SN 0022-2291
EI 1573-7357
J9 J LOW TEMP PHYS
JI J. Low Temp. Phys.
PD AUG
PY 2014
VL 176
IS 3-4
BP 511
EP 517
DI 10.1007/s10909-013-1008-1
PG 7
WC Physics, Applied; Physics, Condensed Matter
SC Physics
GA AK1WY
UT WOS:000338210800059
ER
PT J
AU Faverzani, M
Day, PK
Falferi, P
Ferri, E
Giachero, A
Giordano, C
LeDuc, HG
Marghesin, B
Mezzena, R
Nizzolo, R
Nucciotti, A
AF Faverzani, M.
Day, P. K.
Falferi, P.
Ferri, E.
Giachero, A.
Giordano, C.
LeDuc, H. G.
Marghesin, B.
Mezzena, R.
Nizzolo, R.
Nucciotti, A.
TI Development of Superconducting Microresonators for a Neutrino Mass
Experiment
SO JOURNAL OF LOW TEMPERATURE PHYSICS
LA English
DT Article
DE MKID detectors; Neutrino mass; Holmium
ID KINETIC INDUCTANCE DETECTORS; REDUCTION; ARRAYS; DECAY
AB The determination of the neutrino mass is still an open issue in particle physics. The calorimetric measurement of the energy released in a nuclear beta decay allows to measure all the released energy, except the fraction carried away by the neutrino: a finite neutrino mass m causes the energy spectrum to be truncated at Q m, where Q is the transition energy. The electron capture of Ho (Q 2.5 keV) results to be an ideal decay. In order to achieve enough statistics, a large number of detectors (10) is required. Superconducting microwave microresonators are detectors suitable for large-scale multiplexed frequency domain readout, with theoretical energy and time resolution of eV and s. Our aim is to develop arrays of microresonator detectors applicable to the calorimetric measurement of the energy spectra of Ho. Currently, a study aimed to the selection of the best design and material for the detectors is in progress. In this contribution, a comparison between the measurements (critical temperature, gap parameter, quasiparticle recombination time and X-ray energy spectra) made with stoichiometric, sub-stoichiometric TiN and Ti/TiN multilayer films are presented.
C1 [Faverzani, M.; Ferri, E.; Giachero, A.; Nizzolo, R.; Nucciotti, A.] Univ Milano Bicocca, Milan, Italy.
[Faverzani, M.; Ferri, E.; Giachero, A.; Nucciotti, A.] INFN Milano Bicocca, Milan, Italy.
[Day, P. K.; LeDuc, H. G.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Falferi, P.] CNR Fdn Bruno Kessler, Ist Foton & Nanotecnol, Trento, Italy.
[Giordano, C.; Marghesin, B.] FBK, Trento, Italy.
[Mezzena, R.] Univ Trento, Dipartimento Fis, Trento, Italy.
RP Faverzani, M (reprint author), Univ Milano Bicocca, Milan, Italy.
EM marco.faverzani@mib.infn.it
RI Giachero, Andrea/I-1081-2013; Nucciotti, Angelo/I-8888-2012; Ferri,
Elena/L-8531-2014; Falferi, Paolo/C-3439-2015; Mezzena,
Renato/K-1802-2015; Faverzani, Marco/K-3865-2016
OI Giachero, Andrea/0000-0003-0493-695X; Nucciotti,
Angelo/0000-0002-8458-1556; Ferri, Elena/0000-0003-1425-3669; Falferi,
Paolo/0000-0002-1929-4710; Mezzena, Renato/0000-0001-9891-0472;
Faverzani, Marco/0000-0001-8119-2953
FU Fondazione Cariplo through project Development of Microresonator
Detectors for Neutrino Physics [2010-2351]
FX This work is supported by Fondazione Cariplo through the project
Development of Microresonator Detectors for Neutrino Physics (Grant
2010-2351).
NR 16
TC 3
Z9 3
U1 0
U2 11
PU SPRINGER/PLENUM PUBLISHERS
PI NEW YORK
PA 233 SPRING ST, NEW YORK, NY 10013 USA
SN 0022-2291
EI 1573-7357
J9 J LOW TEMP PHYS
JI J. Low Temp. Phys.
PD AUG
PY 2014
VL 176
IS 3-4
BP 530
EP 537
DI 10.1007/s10909-013-1051-y
PG 8
WC Physics, Applied; Physics, Condensed Matter
SC Physics
GA AK1WY
UT WOS:000338210800062
ER
PT J
AU Hokin, MS
McCammon, D
Morgan, KM
Bandler, SR
Lee, SJ
Moseley, SH
Smith, SJ
AF Hokin, M. S.
McCammon, D.
Morgan, K. M.
Bandler, S. R.
Lee, S. J.
Moseley, S. H.
Smith, S. J.
TI Narrow Line X-Ray Calibration Source for High Resolution
Microcalorimeters
SO JOURNAL OF LOW TEMPERATURE PHYSICS
LA English
DT Article
DE Microcalorimeters; Calibration; Fiber-optics; Lasers; X-ray detectors
AB We are developing a narrow line calibration source for use with X-ray microcalorimeters. At energies below 300 eV fluorescent lines are intrinsically broad, making calibration of high resolution detectors difficult. This source consists of a 405 nm (3 eV) laser diode coupled to an optical fiber. The diode is pulsed to create approximately one hundred photons in a few microseconds. If the pulses are short compared to the rise time of the detector, they will be detected as single events with a total energy in the soft X-ray range. Poisson fluctuations in photon number per pulse create a comb of X-ray lines with 3 eV spacing, so detectors with energy resolution better than 2 eV are required to resolve the individual lines. Our currently unstabilized diode has a multimode width less than 1 nm, giving a 300 eV event a FWHM less than 0.1 eV. By varying the driving voltage, or pulse width, the source can produce a comb centered on a wide range of energies. The calibration events are produced at precisely known times. This allows continuous calibration of a flight mission without contaminating the observed spectrum and with minimal deadtime.
C1 [Hokin, M. S.; McCammon, D.; Morgan, K. M.] Univ Wisconsin, Dept Phys, Madison, WI 53706 USA.
[Bandler, S. R.; Lee, S. J.; Moseley, S. H.; Smith, S. J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Hokin, MS (reprint author), Univ Wisconsin, Dept Phys, 1150 Univ Ave, Madison, WI 53706 USA.
EM mhokin@wisc.edu
RI Smith, Stephen/B-1256-2008; Bandler, Simon/A-6258-2010; Lee, Sang
Jun/A-3892-2015; Morgan, Kelsey/J-5053-2016
OI Smith, Stephen/0000-0003-4096-4675; Bandler, Simon/0000-0002-5112-8106;
Lee, Sang Jun/0000-0002-8199-3993; Morgan, Kelsey/0000-0002-6597-1030
FU NASA [NNX09AF09G]; NASA office of the Chief Technologist's Space
Technology Research Fellowship
FX This work was supported in part by NASA grant NNX09AF09G. K.M. Morgan is
supported by a NASA office of the Chief Technologist's Space Technology
Research Fellowship.
NR 2
TC 1
Z9 1
U1 0
U2 5
PU SPRINGER/PLENUM PUBLISHERS
PI NEW YORK
PA 233 SPRING ST, NEW YORK, NY 10013 USA
SN 0022-2291
EI 1573-7357
J9 J LOW TEMP PHYS
JI J. Low Temp. Phys.
PD AUG
PY 2014
VL 176
IS 3-4
BP 566
EP 570
DI 10.1007/s10909-013-1029-9
PG 5
WC Physics, Applied; Physics, Condensed Matter
SC Physics
GA AK1WY
UT WOS:000338210800067
ER
PT J
AU Akamatsu, H
Gottardi, L
Adams, J
Bandler, S
Bruijn, M
Chervenak, J
Eckart, M
Finkbeiner, F
den Hartog, R
Hoevers, H
Kelley, R
Kilbourne, C
van der Kuur, J
van den Linden, AJ
Porter, F
Sadleir, J
Smith, S
Kiviranta, M
AF Akamatsu, H.
Gottardi, L.
Adams, J.
Bandler, S.
Bruijn, M.
Chervenak, J.
Eckart, M.
Finkbeiner, F.
den Hartog, R.
Hoevers, H.
Kelley, R.
Kilbourne, C.
van der Kuur, J.
van den Linden, A. J.
Porter, F.
Sadleir, J.
Smith, S.
Kiviranta, M.
TI Performance of TES X-ray Microcalorimeters with AC Bias Read-Out at MHz
Frequencies
SO JOURNAL OF LOW TEMPERATURE PHYSICS
LA English
DT Article
DE X-ray; Transition edge sensor; Microcalorimeter
ID ABSORBER DESIGN
AB At SRON we are developing Frequency Domain Multiplexing for the read-out of superconducting transition edge sensor microcalorimeters for future X-ray astrophysical missions. We will report on the performance of Goddard Space Flight Center pixels under AC bias in the MHz frequency range. Superconducting flux transformers are used to improve the impedance matching between the low ohmic TESs and the SQUID. We connected 5 pixels to the LC filters with resonant frequencies ranging between 1 and 5 MHz. For X-ray photons of 6 keV we measured a best X-ray energy resolution of 3.6 eV at 1.4 MHz, consistent with the integrated Noise Equivalent Power. In addition, we improved the electrical circuit by optimizing the coupling ratio of the impedance matching transformer. In addition, we improved electrical circuit for impedance matching; modified transformer coupling ratio. As a result, we got the integrated noise equivalent power resolution of 2.7 eV at 2.5 MHz. A characterization of the detector response as a function of the AC bias voltage, bias frequency and the applied magnetic field is presented.
C1 [Akamatsu, H.; Gottardi, L.; Bruijn, M.; den Hartog, R.; Hoevers, H.; van der Kuur, J.; van den Linden, A. J.] SRON Netherlands Inst Space Res, NL-3584 CA Utrecht, Netherlands.
[Adams, J.; Bandler, S.; Chervenak, J.; Eckart, M.; Finkbeiner, F.; Kelley, R.; Kilbourne, C.; Porter, F.; Sadleir, J.; Smith, S.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Kiviranta, M.] VTT, Espoo, Finland.
RP Akamatsu, H (reprint author), SRON Netherlands Inst Space Res, Sorbonnelaan 2, NL-3584 CA Utrecht, Netherlands.
EM h.akamatsu@sron.nl
RI Smith, Stephen/B-1256-2008; Bandler, Simon/A-6258-2010; Porter,
Frederick/D-3501-2012
OI Smith, Stephen/0000-0003-4096-4675; Bandler, Simon/0000-0002-5112-8106;
Porter, Frederick/0000-0002-6374-1119
FU NWO, the Netherlands Organization for Scientific Research
FX The authors would like to thank Martijn Schoemans, Dick Boersma, Marcel
van Litsenburg and Robert Huiting for their precious technical help. We
also thank an anonymous referees for constructive comments. SRON is
supported financially by NWO, the Netherlands Organization for
Scientific Research.
NR 10
TC 3
Z9 3
U1 0
U2 8
PU SPRINGER/PLENUM PUBLISHERS
PI NEW YORK
PA 233 SPRING ST, NEW YORK, NY 10013 USA
SN 0022-2291
EI 1573-7357
J9 J LOW TEMP PHYS
JI J. Low Temp. Phys.
PD AUG
PY 2014
VL 176
IS 3-4
BP 591
EP 596
DI 10.1007/s10909-014-1130-8
PG 6
WC Physics, Applied; Physics, Condensed Matter
SC Physics
GA AK1WY
UT WOS:000338210800071
ER
PT J
AU Lee, SJ
Bandler, SR
Busch, SE
Adams, JS
Chervenak, JA
Eckart, ME
Ewin, AJ
Finkbeiner, FM
Kelley, RL
Kilbourne, CA
Porst, JP
Porter, FS
Sadleir, JE
Smith, SJ
Wassel, EJ
AF Lee, S. J.
Bandler, S. R.
Busch, S. E.
Adams, J. S.
Chervenak, J. A.
Eckart, M. E.
Ewin, A. J.
Finkbeiner, F. M.
Kelley, R. L.
Kilbourne, C. A.
Porst, J. -P.
Porter, F. S.
Sadleir, J. E.
Smith, S. J.
Wassel, E. J.
TI High Count-Rate Studies of Small-Pitch Transition-Edge Sensor X-ray
Microcalorimeters
SO JOURNAL OF LOW TEMPERATURE PHYSICS
LA English
DT Article
DE Low temperature detector; Transition-edge sensor; X-ray spectroscopy;
High count-rate; Signal processing
AB We are developing kilo-pixel arrays of small-pitch transition-edge sensors for high spectral-resolving, high count-rate applications in astrophysics and solar physics measurements. We have fabricated and tested pixels that are m in size on a silicon substrate with an X-ray flux of counts per second (cps) per pixel. The X-ray pulses were recorded and analyzed in various ways to obtain high throughput with good energy resolution. We have demonstrated 2.3 eV FWHM resolution with 99.6 % throughput for a 6-keV X-ray flux of 100 cps.
C1 [Lee, S. J.; Bandler, S. R.; Busch, S. E.; Adams, J. S.; Chervenak, J. A.; Eckart, M. E.; Ewin, A. J.; Finkbeiner, F. M.; Kelley, R. L.; Kilbourne, C. A.; Porst, J. -P.; Porter, F. S.; Sadleir, J. E.; Smith, S. J.; Wassel, E. J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Bandler, S. R.] CRESST, College Pk, MD 20742 USA.
[Bandler, S. R.] Univ Maryland, College Pk, MD 20742 USA.
[Adams, J. S.; Eckart, M. E.; Smith, S. J.] CRESST, Baltimore, MD 21250 USA.
[Adams, J. S.; Eckart, M. E.; Smith, S. J.] Univ Maryland Baltimore Cty, Baltimore, MD 21250 USA.
[Finkbeiner, F. M.] Wyle Informat Syst, Mclean, VA 22102 USA.
[Porst, J. -P.] CRESST, Columbia, MD 21044 USA.
[Porst, J. -P.] USRA, Columbia, MD 21044 USA.
[Wassel, E. J.] MEI Technol Inc, Lanham, MD 20706 USA.
RP Lee, SJ (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
EM quantization@gmail.com
RI Smith, Stephen/B-1256-2008; Bandler, Simon/A-6258-2010; Lee, Sang
Jun/A-3892-2015; Porter, Frederick/D-3501-2012
OI Smith, Stephen/0000-0003-4096-4675; Bandler, Simon/0000-0002-5112-8106;
Lee, Sang Jun/0000-0002-8199-3993; Porter, Frederick/0000-0002-6374-1119
FU NASA Postdoctoral Program at Goddard Space Flight Center; NASA
FX This research was supported in part by an appointment to the NASA
Postdoctoral Program at Goddard Space Flight Center (S. J. Lee and S. E.
Busch), administered by Oak Ridge Associated Universities through a
contract with NASA.
NR 14
TC 3
Z9 3
U1 0
U2 7
PU SPRINGER/PLENUM PUBLISHERS
PI NEW YORK
PA 233 SPRING ST, NEW YORK, NY 10013 USA
SN 0022-2291
EI 1573-7357
J9 J LOW TEMP PHYS
JI J. Low Temp. Phys.
PD AUG
PY 2014
VL 176
IS 3-4
BP 597
EP 603
DI 10.1007/s10909-013-1071-7
PG 7
WC Physics, Applied; Physics, Condensed Matter
SC Physics
GA AK1WY
UT WOS:000338210800072
ER
PT J
AU Islam, T
Srivastava, PK
Rico-Ramirez, MA
Dai, Q
Han, DW
Gupta, M
AF Islam, Tanvir
Srivastava, Prashant K.
Rico-Ramirez, Miguel A.
Dai, Qiang
Han, Dawei
Gupta, Manika
TI An exploratory investigation of an adaptive neuro fuzzy inference system
(ANFIS) for estimating hydrometeors from TRMM/TMI in synergy with
TRMM/PR
SO ATMOSPHERIC RESEARCH
LA English
DT Article
DE Liquid water contents; Ice water contents; Global precipitation
measurement (GPM); Rain rate retrieval; Passive microwave radiometry;
Precipitation radar
ID PRECIPITATION RADAR; PROFILING ALGORITHM; CLOUD PROPERTIES; NETWORK
AB The authors have investigated an adaptive neuro fuzzy inference system (ANFIS) for the estimation of hydrometeors from the TRMM microwave imager (TMI). The proposed algorithm, named as Hydro-Rain algorithm, is developed in synergy with the TRMM precipitation radar (PR) observed hydrometeor information. The method retrieves rain rates by exploiting the synergistic relations between the TMI and PR observations in twofold steps. First, the fundamental hydrometeor parameters, liquid water path (LWP) and ice water path (IWP), are estimated from the TMI brightness temperatures. Next, the rain rates are estimated from the retrieved hydrometeor parameters (LWP and IWP). A comparison of the hydrometeor retrievals by the Hydro-Rain algorithm is done with the TRMM PR 2A25 and GPROF 2A12 algorithms. The results reveal that the Hydro-Rain algorithm has good skills in estimating hydrometeor paths LWP and IWP, as well as surface rain rate. An examination of the Hydro-Rain algorithm is also conducted on a super typhoon case, in which the Hydro-Rain has shown very good performance in reproducing the typhoon field. Nevertheless, the passive microwave based estimate of hydrometeors appears to suffer in high rain rate regimes, and as the rain rate increases, the discrepancies with hydrometeor estimates tend to increase as well. (C) 2014 Elsevier B.V. All rights reserved.
C1 [Islam, Tanvir] NOAA, NESDIS, Ctr Weather & Climate Predict, College Pk, MD USA.
[Islam, Tanvir] Colorado State Univ, Cooperat Inst Res Atmosphere, Ft Collins, CO 80523 USA.
[Islam, Tanvir; Srivastava, Prashant K.; Rico-Ramirez, Miguel A.; Dai, Qiang; Han, Dawei] Univ Bristol, Dept Civil Engn, Bristol, Avon, England.
[Srivastava, Prashant K.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Srivastava, Prashant K.] Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20742 USA.
[Gupta, Manika] Indian Inst Technol Delhi, Dept Civil Engn, New Delhi, India.
RP Islam, T (reprint author), NOAA, NESDIS, STAR, Ctr Weather & Climate Predict, 5830 Univ Res Ct, College Pk, MD 20740 USA.
EM tanvir.islam@noaa.gov
RI Islam, Tanvir/F-6922-2011; Rico-Ramirez, Miguel/H-3248-2014;
OI Rico-Ramirez, Miguel/0000-0002-8885-4582; Islam,
Tanvir/0000-0003-2429-3074
NR 20
TC 10
Z9 10
U1 1
U2 12
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 AUG-SEP
PY 2014
VL 145
BP 57
EP 68
DI 10.1016/j.atmosres.2014.03.019
PG 12
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA AJ8UK
UT WOS:000337983100005
ER
PT J
AU Newell, PT
Tsurutani, BT
AF Newell, P. T.
Tsurutani, B. T.
TI Introduction to this special issue: "Sun-Earth system exploration:
Moderate and extreme disturbances"
SO JOURNAL OF ATMOSPHERIC AND SOLAR-TERRESTRIAL PHYSICS
LA English
DT Editorial Material
C1 [Newell, P. T.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA.
[Tsurutani, B. T.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Newell, PT (reprint author), Johns Hopkins Univ, Appl Phys Lab, Johns Hopkins Rd, Laurel, MD 20723 USA.
EM Patrick.Newell@jhuapl.edu
NR 0
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 1364-6826
EI 1879-1824
J9 J ATMOS SOL-TERR PHY
JI J. Atmos. Sol.-Terr. Phys.
PD AUG
PY 2014
VL 115
SI SI
BP 1
EP 1
DI 10.1016/j.jastp.2014.02.004
PG 1
WC Geochemistry & Geophysics; Meteorology & Atmospheric Sciences
SC Geochemistry & Geophysics; Meteorology & Atmospheric Sciences
GA AJ8VR
UT WOS:000337986700001
ER
PT J
AU Mannucci, AJ
Crowley, G
Tsurutani, BT
Verkhoglyadova, OP
Komjathy, A
Stephens, P
AF Mannucci, A. J.
Crowley, G.
Tsurutani, B. T.
Verkhoglyadova, O. P.
Komjathy, A.
Stephens, P.
TI Interplanetary magnetic field B-y control of prompt total electron
content increases during superstorms
SO JOURNAL OF ATMOSPHERIC AND SOLAR-TERRESTRIAL PHYSICS
LA English
DT Article
DE Ionosphere; Geomagnetic storms
ID LOW-LATITUDE IONOSPHERE; TRANSPOLAR POTENTIAL SATURATION; GEOMAGNETIC
STORMS; THERMOSPHERE MODEL; NOVEMBER 2003; HILL MODEL; ELECTRODYNAMICS;
EQUATORIAL; TUTORIAL; CONVECTION
AB Large magnitude increases in ionospheric total electron content (TEC) that occur over 1-3 h on the dayside are a significant manifestation of the main phases of superstorms. For the largest superstorms of solar cycle 23 (based on the Dst index), ground networks of GPS receivers measured peak total electron content increases greater than a factor of 2 relative to quiet time TEC averaged over the broad latitude band +/- 40 degrees for local times 1200-1600 LT. Near 30 degrees latitude, the Halloween storms of October 29-30, 2003 appeared to produce storm-time TEC exceeding quiet time values by a factor of 5 within 2-3 h of storm onset, at 1300 LT. The physical cause of these large positive phase ionospheric storms is usually attributed to prompt penetration electric fields (PPEFs) initiated by Region 1 current closure through the ionosphere (Nopper and Carovillano, 1978 mechanism). An unresolved question is what determines variation of the TEC response for different superstorms. It has been suggested that the cross polar cap potential and Region I currents are significant factors in determining PPEF in the equatorial ionosphere, which are related to the solar wind reconnection electric field estimated by Kan-Lee and others. In this paper, we show evidence that suggests B-y may be a significant factor controlling the TEC response during the main phase of superstorms. We analyzed the interplanetary conditions during the period that TEC was increasing for eight superstorms. We find that increasing daytime TEC during superstorms only occurs for large reconnection electric fields when B-y magnitude is less than B-z. The data suggest that B-z is a far more important factor in the TEC response than the reconnection electric field. We also find that TEC decreases following its peak storm-time value for two superstorms, even though B-z remains large and B-y magnitudes are less than B-z. Such decreases during the geomagnetic disturbance may indicate the role of magnetospheric shielding currents, or of changes in the thermosphere that have developed over the prolonged period of large solar wind electric field. Further analysis is warranted covering a wider range of storm intensities on the role of B-y in affecting the daytime TEC response for a range of storm intensities. (C) 2014 Elsevier Ltd. All rights reserved.
C1 [Mannucci, A. J.; Tsurutani, B. T.; Verkhoglyadova, O. P.; Komjathy, A.] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
[Crowley, G.] Atmospher & Space Technol Res Associates, Boulder, CO USA.
[Stephens, P.] Google Inc, Santa Monica, CA USA.
RP Mannucci, AJ (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
EM anthony.j.mannucci@jpl.nasa.gov
OI Verkhoglyadova, Olga/0000-0002-9295-9539
NR 60
TC 11
Z9 11
U1 3
U2 19
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 1364-6826
EI 1879-1824
J9 J ATMOS SOL-TERR PHY
JI J. Atmos. Sol.-Terr. Phys.
PD AUG
PY 2014
VL 115
SI SI
BP 7
EP 16
DI 10.1016/j.jastp.2014.01.001
PG 10
WC Geochemistry & Geophysics; Meteorology & Atmospheric Sciences
SC Geochemistry & Geophysics; Meteorology & Atmospheric Sciences
GA AJ8VR
UT WOS:000337986700003
ER
PT J
AU Verkhoglyadova, OP
Tsurutani, BT
Mannucci, AJ
Mlynczak, MG
Hunt, LA
Paxton, LJ
AF Verkhoglyadova, O. P.
Tsurutani, B. T.
Mannucci, A. J.
Mlynczak, M. G.
Hunt, L. A.
Paxton, L. J.
TI Ionospheric TEC, thermospheric cooling and Sigma[O/N-2] compositional
changes during the 6-17 March 2012 magnetic storm interval (CAWSES II)
SO JOURNAL OF ATMOSPHERIC AND SOLAR-TERRESTRIAL PHYSICS
LA English
DT Article
DE Ionosphere; Thermosphere; Geomagnetic storms
ID LOW-LATITUDE; SOLAR; MODEL; TIMED/GUVI; SUPERSTORM
AB A series of four geomagnetic storms (the minimum SYM-H similar to-148 nT) occurred during the March 6-17, 2012 in the ascending phase of the solar cycle 24. This interval was selected by CAWSES II for its campaign. The GPS total electron content (TEC) database and JPL's Global Ionospheric Maps (GIM) were used to study vertical TEC (VTEC) for different local times and latitude ranges. The largest response to geomagnetic activity is shown in increases of the low-latitude dayside VTEC. Several GPS sites feature post-afternoon VTEC "bite-outs". During Sudden Impulse (SI+) event on March 8th a peak daytime VTEC restores to about quiet-time values. It is shown that the TIMED/SABER zonal flux of nitric oxide (NO) infrared cooling radiation correlates well with auroral heating. A factor of similar to 5 cooling increase is noted in some storms. The cooling radiation intensifies in the auroral zone and spreads towards the equator. Effects of the storm appear at lower latitudes similar to 18.6 h later. The column density ratio Sigma[O/N-2] is analyzed based on TIMED/GUVI measurements. Both increases (at low latitudes) and decreases (from auroral to middle latitudes) in the ratio occurs during the geomagnetic storms. We suggest that the column density ratio could be enhanced at low to middle latitudes on the dayside partially due to the superfountain effect (atomic oxygen uplift due to ion-neutral drag). It is suggested that decreases in the [O/N-2] ratio at high to middle-latitudes may be caused by high thermospheric temperatures. During SI+ s, there is an increase in Sigma[O/N-2] ratio at auroral latitudes. (C) 2013 Elsevier Ltd. All rights reserved.
C1 [Verkhoglyadova, O. P.; Tsurutani, B. T.; Mannucci, A. J.] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
[Verkhoglyadova, O. P.] UAH, Ctr Space & Aeron Res, Huntsville, AL USA.
[Mlynczak, M. G.] NASA, Langley Res Ctr, Hampton, VA 23665 USA.
[Hunt, L. A.] Sci Syst & Applicat Inc, Hampton, VA USA.
[Paxton, L. J.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD USA.
RP Verkhoglyadova, OP (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
EM Olga.Verkhoglyadova@jpl.nasa.gov
RI Paxton, Larry/D-1934-2015;
OI Paxton, Larry/0000-0002-2597-347X; Verkhoglyadova,
Olga/0000-0002-9295-9539
NR 42
TC 4
Z9 4
U1 0
U2 7
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 1364-6826
EI 1879-1824
J9 J ATMOS SOL-TERR PHY
JI J. Atmos. Sol.-Terr. Phys.
PD AUG
PY 2014
VL 115
SI SI
BP 41
EP 51
DI 10.1016/j.jastp.2013.11.009
PG 11
WC Geochemistry & Geophysics; Meteorology & Atmospheric Sciences
SC Geochemistry & Geophysics; Meteorology & Atmospheric Sciences
GA AJ8VR
UT WOS:000337986700007
ER
PT J
AU Moore, TE
Fok, MC
Garcia-Sage, K
AF Moore, T. E.
Fok, M. -C.
Garcia-Sage, K.
TI The ionospheric outflow feedback loop
SO JOURNAL OF ATMOSPHERIC AND SOLAR-TERRESTRIAL PHYSICS
LA English
DT Article
DE Ionosphere; Feedback; Magnetosphere
ID ION OUTFLOW; MAGNETOSPHERE; POLAR; FIELD; WIND; CIRCULATION; PLASMA;
REGION; EISCAT; WAVES
AB Following a long period of observation and investigation beginning in the early 1970s, it has been firmly established that Earth's magnetosphere is defined as much by the geogenic plasma within it as by the geomagnetic field. This plasma is not confined to the ionosphere proper, defined as the region within a few density scale heights of the F-region plasma density peak. Rather, it fills the flux tubes on which it is created, and circulates throughout the magnetosphere in a pattern driven by solar wind plasma that becomes magnetically connected to the ionosphere by reconnection through the dayside magnetopause. Under certain solar wind conditions, plasma and field energy is stored in the magnetotail rather than being smoothly recirculated back to the dayside. Its release into the downstream solar wind is produced by magnetotail disconnection of stored plasma and fields both continuously and in the form of discrete plasmoids, with associated generation of energetic Earthward-moving bursty bulk flows and injection fronts. A new generation of global circulation models is showing us that outflowing ionospheric plasmas, especially O+, load the system in a different way than the resistive F-region load of currents dissipating energy in the plasma and atmospheric neutral gas. The extended ionospheric load is reactive to the primary dissipation, forming a time-delayed feedback loop within the system. That sets up or intensifies bursty transient behaviors that would be weaker or absent if the ionosphere did not "strike back" when stimulated. Understanding this response appears to be a necessary, if not sufficient, condition for us to gain accurate predictive capability for space weather. However, full predictive understanding of outflow and incorporation into global simulations requires a clear observational and theoretical identification of the causal mechanisms of the outflows. This remains elusive and requires a dedicated mission effort. Published by Elsevier Ltd.
C1 [Moore, T. E.; Fok, M. -C.; Garcia-Sage, K.] NASA, Goddard SFC, Greenbelt, MD 20771 USA.
RP Moore, TE (reprint author), NASA, Goddard SFC, Greenbelt, MD 20771 USA.
FU NASA Postdoctoral Program; Magnetospheric Multiscale (MMS) at NASA
Goddard Space Flight Center
FX The authors gratefully acknowledge support by the NASA Postdoctoral
Program, and the Magnetospheric Multiscale (MMS) at NASA Goddard Space
Flight Center.
NR 37
TC 7
Z9 7
U1 2
U2 5
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 1364-6826
EI 1879-1824
J9 J ATMOS SOL-TERR PHY
JI J. Atmos. Sol.-Terr. Phys.
PD AUG
PY 2014
VL 115
SI SI
BP 59
EP 66
DI 10.1016/j.jastp.2014.02.002
PG 8
WC Geochemistry & Geophysics; Meteorology & Atmospheric Sciences
SC Geochemistry & Geophysics; Meteorology & Atmospheric Sciences
GA AJ8VR
UT WOS:000337986700009
ER
PT J
AU Keesee, AM
Elfritz, JG
Fok, MC
McComas, DJ
Scime, EE
AF Keesee, A. M.
Elfritz, J. G.
Fok, M. -C.
McComas, D. J.
Scime, E. E.
TI Superposed epoch analyses of ion temperatures during CME- and
CIR/HSS-driven storms
SO JOURNAL OF ATMOSPHERIC AND SOLAR-TERRESTRIAL PHYSICS
LA English
DT Article
DE Magnetosphere; Geomagnetic storm; CME; High speed stream; Corotating
interaction region; Ion temperature
ID PLASMA SHEET; GEOMAGNETIC STORMS; TWINS; MODEL
AB Coronal mass ejections (CMEs) and corotating interaction regions associated with high speed solar wind streams (CIR/HSSs) drive geomagnetic storms in the terrestrial magnetosphere. Each type of storm driver yields different dynamics of storm evolution. We present results from comparative superposed epoch analyses of global ion temperatures calculated from TWINS energetic neutral atom (ENA) data and simulations using the comprehensive ring current model (CRCM). During the June 2008-April 2012 timeframe, 48 geomagnetic storms (minimum Dst <= -40 nT) occurred. Of these, 21 storms were CME-driven and 15 were driven by CIR/HSSs. Superposed epoch analysis results demonstrate that ion temperatures increase during the recovery phase of CIR/HSS-driven storms, while ions are rapidly heated at the commencement of CME-driven storms then cool over the main phase, particularly for intense (minimum Dst <= -78 nT) CME-driven storms. Higher energy ions are convected to lower L-shells during CME-driven storms, while CIR/HSS-driven storms tend to have average ion temperatures that are higher on the dayside than nightside. (C) 2013 Elsevier Ltd. All rights reserved.
C1 [Keesee, A. M.; Elfritz, J. G.; Scime, E. E.] W Virginia Univ, Dept Phys, Morgantown, WV 26506 USA.
[Fok, M. -C.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[McComas, D. J.] SW Res Inst, San Antonio, TX 78228 USA.
[McComas, D. J.] Univ Texas San Antonio, San Antonio, TX 78249 USA.
RP Keesee, AM (reprint author), W Virginia Univ, Dept Phys, Morgantown, WV 26506 USA.
EM amy.keesee@mail.wvu.edu
RI Keesee, Amy/J-8194-2014
OI Keesee, Amy/0000-0002-9719-3229
FU NASA EPSCoR [NNX10AN08A]; NSF [AGS-1113478]; WVU
FX This work was carried out as a part of the TWINS NASA Explorer mission;
work at WVU was supported under subcontract to the Southwest Research
Institute, NASA EPSCoR grant NNX10AN08A and NSF grant AGS-1113478. We
would like to thank members of the TWINS science team for helpful
discussions regarding the TWINS ENA data. We gratefully acknowledge the
use of solar wind data and geomagnetic indices provided by OMNIWeb and
Kyoto World Data Center for Geomagnetism.
NR 27
TC 7
Z9 7
U1 0
U2 5
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 1364-6826
EI 1879-1824
J9 J ATMOS SOL-TERR PHY
JI J. Atmos. Sol.-Terr. Phys.
PD AUG
PY 2014
VL 115
SI SI
BP 67
EP 78
DI 10.1016/j.jastp.2013.08.009
PG 12
WC Geochemistry & Geophysics; Meteorology & Atmospheric Sciences
SC Geochemistry & Geophysics; Meteorology & Atmospheric Sciences
GA AJ8VR
UT WOS:000337986700010
ER
PT J
AU Huang, YS
Richmond, AD
Deng, Y
Chamberlin, PC
Qian, LY
Solomon, SC
Roble, RG
Xiao, Z
AF Huang, Yanshi
Richmond, Arthur D.
Deng, Yue
Chamberlin, Phillip C.
Qian, Liying
Solomon, Stanley C.
Roble, Raymond G.
Xiao, Zuo
TI Wavelength dependence of solar irradiance enhancement during X-class
flares and its influence on the upper atmosphere
SO JOURNAL OF ATMOSPHERIC AND SOLAR-TERRESTRIAL PHYSICS
LA English
DT Article
DE Solar flare; FISM; TIE-GCM
ID GENERAL-CIRCULATION MODEL; EUV EXPERIMENT; THERMOSPHERE; IONOSPHERE
AB The wavelength dependence of solar irradiance enhancement during flare events is one of the important factors in determining how the Thermosphere-Ionosphere (T-I) system responds to flares. To investigate the wavelength dependence of flare enhancement, the Flare Irradiance Spectral Model (FISM) was run for 61 X-class flares. The absolute and the percentage increases of solar irradiance at flare peaks, compared to pre-flare conditions, have clear wavelength dependences. The 0-14 nm irradiance increases much more (similar to 680% on average) than that in the 14-25 nm waveband (similar to 65% on average), except at 24 nm (similar to 220%). The average percentage increases for the 25-105 nm and 122-190 nm wavebands are similar to 120% and similar to 35%, respectively. The influence of 6 different wavebands (0-14 nm, 14-25 nm, 25-105 nm, 105-120 nm, 121.56 nm, and 122-175 nm) on the thermosphere was examined for the October 28th, 2003 flare (X17-class) event by coupling FISM with the National Center for Atmospheric Research (NCAR) Thermosphere-Ionosphere-Electrodynamics General Circulation Model (TIE-GCM) under geomagnetically quiet conditions (Kp=1). While the enhancement in the 0-14 nm waveband caused the largest enhancement of the globally integrated solar heating, the impact of solar irradiance enhancement on the thermosphere at 400 km is largest for the 25-105 nm waveband (EUV), which accounts for about 33 K of the total 45 K temperature enhancement, and similar to 7.4% of the total similar to 11.5% neutral density enhancement. The effect of 122-175 nm flare radiation on the thermosphere is rather small. The study also illustrates that the high-altitude thermospheric response to the flare radiation at 0-175 nm is almost a linear combination of the responses to the individual wavebands. The upper thermospheric temperature and density enhancements peaked 3-5 h after the maximum flare radiation. (C) 2013 Elsevier Ltd. All rights reserved.
C1 [Huang, Yanshi] Univ New Mexico, Dept Elect & Comp Engn, Albuquerque, NM 87131 USA.
[Richmond, Arthur D.; Qian, Liying; Solomon, Stanley C.; Roble, Raymond G.] Natl Ctr Atmospher Res, High Altitude Observ, Boulder, CO 80307 USA.
[Deng, Yue] Univ Texas Arlington, Dept Phys, Arlington, TX 76019 USA.
[Chamberlin, Phillip C.] NASA, Goddard Space Flight Ctr, Solar Phys Lab, Greenbelt, MD 20771 USA.
[Xiao, Zuo] Peking Univ, Dept Geophys, Beijing 100871, Peoples R China.
RP Huang, YS (reprint author), Univ New Mexico, Dept Elect & Comp Engn, Albuquerque, NM 87131 USA.
EM huangys@unm.edu; richmond@hao.ucar.edu; yuedeng@uta.edu;
phillip.c.chamberlin@nasa.gov; lqian@ucar.edu; stans@ucar.edu;
roble@hao.ucar.ed; zxiao@pku.eud.cn
RI Solomon, Stanley/J-4847-2012; Chamberlin, Phillip/C-9531-2012;
OI Solomon, Stanley/0000-0002-5291-3034; Chamberlin,
Phillip/0000-0003-4372-7405; Richmond, Arthur/0000-0002-6708-1023
FU National Science Foundation [ATM0955629]; Air Force Office of Scientific
Research [1210429]; National Science Foundation
FX We acknowledge the LASP Interactive Solar Irradiance Data center for
FISM data. This research was supported by the National Science
Foundation through grant ATM0955629 and by the Air Force Office of
Scientific Research through grant 1210429. Part of this work was
conducted while Y.H. and Y.D. were visitors in the Advanced Study
Program at the National Center for Atmospheric Research (NCAR). NCAR is
sponsored by the National Science Foundation.
NR 40
TC 0
Z9 0
U1 0
U2 8
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 1364-6826
EI 1879-1824
J9 J ATMOS SOL-TERR PHY
JI J. Atmos. Sol.-Terr. Phys.
PD AUG
PY 2014
VL 115
SI SI
BP 87
EP 94
DI 10.1016/j.jastp.2013.10.011
PG 8
WC Geochemistry & Geophysics; Meteorology & Atmospheric Sciences
SC Geochemistry & Geophysics; Meteorology & Atmospheric Sciences
GA AJ8VR
UT WOS:000337986700012
ER
PT J
AU Pendyala, VRR
Jacobs, G
Ma, WP
Klettlinger, JLS
Yen, CH
Davis, BH
AF Pendyala, Venkat Ramana Rao
Jacobs, Gary
Ma, Wenping
Klettlinger, Jennifer L. S.
Yen, Chia H.
Davis, Burtron H.
TI Fischer-Tropsch synthesis: Effect of catalyst particle (sieve) size
range on activity, selectivity, and aging of a Pt promoted Co/Al2O3
catalyst
SO CHEMICAL ENGINEERING JOURNAL
LA English
DT Article
DE Fischer-Tropsch synthesis; Cobalt catalysts; Sieve size; Activity;
Selectivity
ID CO/SIO2 CATALYSTS; COBALT CATALYSTS; SUPPORT; DISPERSION; REDUCIBILITY
AB The effect of cobalt-alumina catalyst particle (sieve) size range on the performance of a traditional cobalt catalyst (platinum promoted cobalt/alumina) was investigated during Fischer-Tropsch synthesis (FTS) using a continuously stirred tank reactor (CSTR). In this study, the catalyst was sieved into four different size ranges: 20-63, 63-106, 106-180 and 180-355 mu m. CO conversion varied with varying sieve size range under similar reaction conditions. With increasing catalyst sieve size, the CO conversion decreased, except for the smallest sieve size range (20-63 mu m). These results are consistent with the view that, for the larger sieve size range, losses in CO conversion beyond catalyst aging may be explained by filling of the interior of the catalyst particle with heavy wax, thereby blocking available catalytically active sites. The adverse selectivities are directly the result of significant deactivation, since in FT synthesis, selectivity is a function of CO conversion. The loss in CO conversion for the 20-63 mu m range catalyst was higher compared to the other three catalysts; due to the presence of heavy wax (Polywax 3000), the results suggest that the small particles tended to flocculate to larger clusters or were small enough to move at the speed of the liquid. (C) 2014 Elsevier B.V. All rights reserved.
C1 [Pendyala, Venkat Ramana Rao; Jacobs, Gary; Ma, Wenping; Davis, Burtron H.] Univ Kentucky, Ctr Appl Energy Res, Lexington, KY 40511 USA.
[Klettlinger, Jennifer L. S.; Yen, Chia H.] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA.
RP Davis, BH (reprint author), Univ Kentucky, Ctr Appl Energy Res, 2540 Res Pk Dr, Lexington, KY 40511 USA.
EM burtron.davis@uky.edu
RI Jacobs, Gary/M-5349-2015
OI Jacobs, Gary/0000-0003-0691-6717
FU Commonwealth of Kentucky (USA); NASA (USA) [NNX11A175A]
FX This work carried out at the CAER was supported by the Commonwealth of
Kentucky (USA) and a NASA (USA) grant (Relating FTS catalyst properties
to performance no: NNX11A175A).
NR 20
TC 6
Z9 6
U1 7
U2 53
PU ELSEVIER SCIENCE SA
PI LAUSANNE
PA PO BOX 564, 1001 LAUSANNE, SWITZERLAND
SN 1385-8947
EI 1873-3212
J9 CHEM ENG J
JI Chem. Eng. J.
PD AUG 1
PY 2014
VL 249
BP 279
EP 284
DI 10.1016/j.cej.2014.03.100
PG 6
WC Engineering, Environmental; Engineering, Chemical
SC Engineering
GA AJ3GI
UT WOS:000337554100033
ER
PT J
AU Fonollosa, J
Rodriguez-Lujan, I
Shevade, AV
Homer, ML
Ryan, MA
Huerta, R
AF Fonollosa, Jordi
Rodriguez-Lujan, Irene
Shevade, Abhijit V.
Homer, Margie L.
Ryan, Margaret A.
Huerta, Ramon
TI Human activity monitoring using gas sensor arrays
SO SENSORS AND ACTUATORS B-CHEMICAL
LA English
DT Article
DE Activity monitoring; Gas sensors; e-Nose; Support vector machines;
Remote sensing; Home monitoring
ID HOME GAIT ASSESSMENT; PHYSICAL-ACTIVITY; ELECTRONIC NOSE; RECOGNITION;
SYSTEM; CALIBRATION; REGRESSION; NETWORKS
AB A chemical detection system made of a gas sensor array and algorithms intended to monitor human activity was tested in a NASA spacecraft cabin simulator. Such a chemical-based monitoring system, if extended to home settings, would allow the autonomous detection of emergency situations, thereby postponing the moving of elderly people to assisted living facilities and improving their quality of life. Moreover, in contrast to other monitoring systems based on wearable sensors or video cameras, a monitoring system based on measuring changes in air composition induced by human activities would be non-invasive and would not raise privacy concerns when installed in homes. The third generation of the JPL sensor array was adapted in a small, compact and portable system and deployed in a spacecraft-like room for four weeks while volunteers were performing daily routines. The system was able to predict the total number of people and the level of activity performed in the room, while detecting unexpectedly high concentrations of volatiles. (C) 2014 Elsevier B.V. All rights reserved.
C1 [Fonollosa, Jordi; Rodriguez-Lujan, Irene; Huerta, Ramon] Univ Calif San Diego, BioCircuits Inst, La Jolla, CA 92093 USA.
[Shevade, Abhijit V.; Homer, Margie L.; Ryan, Margaret A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Fonollosa, J (reprint author), Univ Calif San Diego, BioCircuits Inst, La Jolla, CA 92093 USA.
EM fonollosa@ucsd.edu
RI Huerta, Ramon/J-4316-2012; Huerta, Ramon/C-9296-2013; Rodriguez-Lujan,
Irene/E-8619-2016; Fonollosa, Jordi/L-2303-2014
OI Huerta, Ramon/0000-0003-3925-5169; Huerta, Ramon/0000-0003-3925-5169;
Rodriguez-Lujan, Irene/0000-0001-9512-9162; Fonollosa,
Jordi/0000-0001-8854-8588
FU Jet Propulsion LaboratoryJet Propulsion Laboratory [2012-1455933]
FX This work has been supported by the Jet Propulsion Laboratory under the
contract number 2012-1455933. The authors want to dedicate this paper to
the memory of their former colleague and friend at UCSD, Dr. Alexander
Vergara, who passed away in March 2014.
NR 45
TC 7
Z9 7
U1 6
U2 48
PU ELSEVIER SCIENCE SA
PI LAUSANNE
PA PO BOX 564, 1001 LAUSANNE, SWITZERLAND
SN 0925-4005
J9 SENSOR ACTUAT B-CHEM
JI Sens. Actuator B-Chem.
PD AUG
PY 2014
VL 199
BP 398
EP 402
DI 10.1016/j.snb.2014.03.102
PG 5
WC Chemistry, Analytical; Electrochemistry; Instruments & Instrumentation
SC Chemistry; Electrochemistry; Instruments & Instrumentation
GA AI5AO
UT WOS:000336878000054
ER
PT J
AU Kramar, M
Airapetian, V
Mikic, Z
Davila, J
AF Kramar, M.
Airapetian, V.
Mikic, Z.
Davila, J.
TI 3D Coronal Density Reconstruction and Retrieving the Magnetic Field
Structure during Solar Minimum
SO SOLAR PHYSICS
LA English
DT Article
DE Corona, quiet, structures; Magnetic fields, corona
ID EMISSION-LINE POLARIZATION; WHITE-LIGHT IMAGES; WHOLE SUN MONTH;
ELECTRON-DENSITY; RADIOLOGICAL APPLICATIONS; VECTOR TOMOGRAPHY; MHD
MODEL; REPRESENTATION; CALIBRATION; INTEGRALS
AB Measurement of the coronal magnetic field is a crucial ingredient in understanding the nature of solar coronal phenomena at all scales. We employed STEREO/COR1 data obtained during a deep minimum of solar activity in February 2008 (Carrington Rotation CR 2066) to retrieve and analyze the three-dimensional (3D) coronal electron density in the range of heights from 1.5 to 4 R-aS (TM) using a tomography method. With this, we qualitatively deduced structures of the coronal magnetic field. The 3D electron-density analysis is complemented by the 3D STEREO/EUVI emissivity in the 195 band obtained by tomography for the same CR. A global 3D MHD model of the solar corona was used to relate the reconstructed 3D density and emissivity to open/closed magnetic-field structures. We show that the density-maximum locations can serve as an indicator of current-sheet position, while the locations of the density-gradient maximum can be a reliable indicator of coronal-hole boundaries. We find that the magnetic-field configuration during CR 2066 has a tendency to become radially open at heliocentric distances greater than 2.5 R-aS (TM). We also find that the potential-field model with a fixed source surface is inconsistent with the boundaries between the regions with open and closed magnetic-field structures. This indicates that the assumption of the potential nature of the coronal global magnetic field is not satisfied even during the deep solar minimum. Results of our 3D density reconstruction will help to constrain solar coronal-field models and test the accuracy of the magnetic-field approximations for coronal modeling.
C1 [Kramar, M.] Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA.
[Kramar, M.; Airapetian, V.; Davila, J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Mikic, Z.] Predict Sci Inc, San Diego, CA 92121 USA.
RP Kramar, M (reprint author), Catholic Univ Amer, Dept Phys, 620 Michigan Ave NE, Washington, DC 20064 USA.
EM kramar@cua.edu
FU NASA [NNG11PL10A 670.008, SCEX22013D]; NSF [AGS0819971]
FX The work of MK has been supported by the NASA Cooperative Agreement
NNG11PL10A 670.008 to the Catholic University of America and NSF
National Space Weather Program grant AGS0819971. VA acknowledges support
from NASA grant SCEX22013D. The authors thank the anonymous referee for
the insightful review of the manuscript.
NR 55
TC 8
Z9 8
U1 0
U2 11
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0038-0938
EI 1573-093X
J9 SOL PHYS
JI Sol. Phys.
PD AUG
PY 2014
VL 289
IS 8
BP 2927
EP 2944
DI 10.1007/s11207-014-0525-7
PG 18
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AH7SS
UT WOS:000336334900007
ER
PT J
AU Panesar, NK
Innes, DE
Schmit, DJ
Tiwari, SK
AF Panesar, N. K.
Innes, D. E.
Schmit, D. J.
Tiwari, S. K.
TI On the Structure and Evolution of a Polar Crown Prominence/Filament
System
SO SOLAR PHYSICS
LA English
DT Article
DE Prominences, quiescent; Prominences, dynamics; Corona, coronal cavities
ID CORONAL MASS EJECTIONS; SOLAR PROMINENCES; QUIESCENT PROMINENCES;
MAGNETIC-STRUCTURE; FILAMENT; CAVITY; DYNAMICS; HINODE; MODELS; FIELDS
AB Polar crown prominences, that partially circle the Sun's poles between 60A degrees and 70A degrees latitude, are made of chromospheric plasma. We aim to diagnose the 3D dynamics of a polar crown prominence using high-cadence EUV images from the Solar Dynamics Observatory (SDO)/AIA at 304, 171, and 193 and the Ahead spacecraft of the Solar Terrestrial Relations Observatory (STEREO-A)/EUVI at 195 . Using time series across specific structures, we compare flows across the disk in 195 with the prominence dynamics seen on the limb. The densest prominence material forms vertical columns that are separated by many tens of Mm and connected by dynamic bridges of plasma that are clearly visible in 304/171 two-colour images. We also observe intermittent but repetitious flows with velocity 15 km s(-1) in the prominence that appear to be associated with EUV bright points on the solar disk. The boundary between the prominence and the overlying cavity appears as a sharp edge. We discuss the structure of the coronal cavity seen both above and around the prominence. SDO/HMI and GONG magnetograms are used to infer the underlying magnetic topology. The evolution and structure of the prominence with respect to the magnetic field seems to agree with the filament-linkage model.
C1 [Panesar, N. K.; Innes, D. E.; Schmit, D. J.; Tiwari, S. K.] Max Planck Inst Sonnensyst Forsch, D-37077 Gottingen, Germany.
[Panesar, N. K.] Inst Astrophys Gottingen, Fak Phys, D-37077 Gottingen, Germany.
[Tiwari, S. K.] NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA.
RP Panesar, NK (reprint author), Max Planck Inst Sonnensyst Forsch, Justus von Liebig Weg 3, D-37077 Gottingen, Germany.
EM panesar@mps.mpg.de
FU NASA
FX We would like to thank the referee for his/her constructive comments.
SDO data are courtesy of the NASA/SDO AIA and HMI science teams. STEREO
data are courtesy of the STEREO Sun Earth Connection Coronal and
Heliospheric Investigation (SECCHI) team. GONG magnetogram data obtained
by the Global Oscillation Network Group (GONG) project, managed by the
National Solar Observatory, which is operated by AURA, Inc. under a
cooperative agreement with the National Science Foundation. NKP
acknowledges the facilities provided by the MPS. One of the authors,
SKT, is supported by an appointment to the NASA Postdoctoral Program at
the NASA Marshall Space Flight Center, administered by Oak Ridge
Associated Universities through a contract with NASA.
NR 65
TC 2
Z9 2
U1 0
U2 3
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0038-0938
EI 1573-093X
J9 SOL PHYS
JI Sol. Phys.
PD AUG
PY 2014
VL 289
IS 8
BP 2971
EP 2991
DI 10.1007/s11207-014-0504-z
PG 21
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AH7SS
UT WOS:000336334900010
ER
PT J
AU Richardson, IG
von Rosenvinge, TT
Cane, HV
Christian, ER
Cohen, CMS
Labrador, AW
Leske, RA
Mewaldt, RA
Wiedenbeck, ME
Stone, EC
AF Richardson, I. G.
von Rosenvinge, T. T.
Cane, H. V.
Christian, E. R.
Cohen, C. M. S.
Labrador, A. W.
Leske, R. A.
Mewaldt, R. A.
Wiedenbeck, M. E.
Stone, E. C.
TI > 25 MeV Proton Events Observed by the High Energy Telescopes on the
STEREO A and B Spacecraft and/or at Earth During the First similar to
aEuro parts per thousand Seven Years of the STEREO Mission
SO SOLAR PHYSICS
LA English
DT Article
DE Solar energetic particles; STEREO; SOHO
ID CORONAL MASS EJECTIONS; SOLAR-FLARE PARTICLES; III RADIO-BURSTS;
INTERPLANETARY SHOCKS; INNER HELIOSPHERE; PEAK INTENSITIES; GNEVYSHEV
GAP; COSMIC-RAYS; 1 AU; PROPAGATION
AB Using observations from the High Energy Telescopes (HETs) on the STEREO A and B spacecraft and similar observations from near-Earth spacecraft, we summarize the properties of more than 200 individual > 25 MeV solar proton events, some detected by multiple spacecraft, that occurred from the beginning of the STEREO mission in October 2006 to December 2013, and provide a catalog of these events and their solar sources and associations. Longitudinal dependencies of the electron and proton peak intensities and delays to onset and peak intensity relative to the solar event have been examined for 25 three-spacecraft particle events. Expressed as Gaussians, peak intensities fall off with longitude with sigma=47 +/- 14(a similar to) for 0.7 -aEuro parts per thousand 4 MeV electrons, and sigma=43 +/- 13(a similar to) for 14 -aEuro parts per thousand 24 MeV protons. Several particle events are discussed in more detail, including one on 3 November 2011, in which similar to aEuro parts per thousand 25 MeV protons filled the inner heliosphere within 90 minutes of the solar event, and another on 7 March 2012, in which we demonstrate that the first of two coronal mass ejections that erupted from an active region within similar to aEuro parts per thousand 1 hour was associated with particle acceleration. Comparing the current Solar Cycle 24 with the previous cycle, the first > 25 MeV proton event was detected at Earth in the current solar cycle around one year after smoothed sunspot minimum, compared with a delay of only two months in Cycle 23. Otherwise, solar energetic particle event occurrence rates were reasonably similar during the rising phases of Cycles 23 and 24. However, the rate declined in 2013, reflecting the decline in sunspot number since the peak in the northern-hemisphere sunspot number in November 2011. Observations in late 2013 suggest that the rate may be rising again in association with an increase in the southern sunspot number.
C1 [Richardson, I. G.; von Rosenvinge, T. T.; Christian, E. R.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Richardson, I. G.] Univ Maryland, CRESST, College Pk, MD 20742 USA.
[Richardson, I. G.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Cane, H. V.] Bruny Isl Radio Spectrometer, Bruny Island, Tas, Australia.
[Cohen, C. M. S.; Labrador, A. W.; Leske, R. A.; Mewaldt, R. A.; Stone, E. C.] CALTECH, Pasadena, CA 91125 USA.
[Wiedenbeck, M. E.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Richardson, IG (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
EM ian.g.richardson@nasa.gov; tycho.t.vonrosenvinge@nasa.gov;
hcane@utas.edu.au; eric.r.christian@nasa.gov; cohen@srl.caltech.edu;
labrador@srl.caltech.edu; ral@srl.caltech.edu; rmewaldt@srl.caltech.edu;
mark.e.wiedenbeck@jpl.nasa.gov; ecs@srl.caltech.edu
OI Richardson, Ian/0000-0002-3855-3634
FU NASA; University of California, Berkeley, under NASA [SA2715-26309,
NAS5-03131]; German Bundesminister fur Wirtschaft through the Deutsches
Zentrum fur Luft- und Raumfahrt (DLR) [50 OC 1302]
FX We thank Janet Luhmann of the University of California, Berkeley, for
her steadfast support as the Principal Investigator of the STEREO/IMPACT
investigation. The work at GSFC, Caltech and JPL was supported by NASA
(Caltech and JPL were funded under subcontract SA2715-26309 from the
University of California, Berkeley, under NASA Contract NAS5-03131). The
LASCO CME catalog at http://cdaw.gsfc.nasa.gov/CME_list/ is generated
and maintained at the CDAW Data Center by NASA and The Catholic
University of America in cooperation with the Naval Research Laboratory.
We particularly appreciate the efforts by S. Yashiro and colleagues to
generate daily summary movies of SOHO and STEREO observations
(http://cdaw.gsfc.nasa.gov/stereo/daily_movies/), which were very
helpful in verifying the solar sources of the SEP events. The CACTUS CME
catalog is maintained by the Solar Influences Data Analysis Center at
the Royal Observatory of Belgium. The SOHO/ERNE data were obtained from
the Space Research Laboratory, University of Turku
(http://www.srl.utu.fi/erne_data/). The SOHO/EPHIN project is supported
under grant No. 50 OC 1302 by the German Bundesminister fur Wirtschaft
through the Deutsches Zentrum fur Luft- und Raumfahrt (DLR). SOHO is a
project of international cooperation between ESA and NASA.
NR 75
TC 54
Z9 54
U1 0
U2 9
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0038-0938
EI 1573-093X
J9 SOL PHYS
JI Sol. Phys.
PD AUG
PY 2014
VL 289
IS 8
BP 3059
EP 3107
DI 10.1007/s11207-014-0524-8
PG 49
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AH7SS
UT WOS:000336334900015
ER
PT J
AU Jouanny, I
Sennour, M
Berger, MH
Filipov, VB
Ievdokyrnova, A
Paderno, VN
Sayir, A
AF Jouanny, I.
Sennour, M.
Berger, M. H.
Filipov, V. B.
Ievdokyrnova, A.
Paderno, V. N.
Sayir, A.
TI Effect of Zr substitution by Ti on growth direction and interface
structure of LaB6-TixZr1-xB2 directionally solidified eutectics
SO JOURNAL OF THE EUROPEAN CERAMIC SOCIETY
LA English
DT Article
DE DSE; Boride; Interfaces; Crystallographic orientation
ID COMPOSITE; CRYSTALLOGRAPHY; DIBORIDES; ZIRCONIUM; FEATURES; ALLOYS
AB Boride ceramics were directionally solidified around LaB6-(TixZr1-x)B-2 eutectic compositions. The directionally solidified rods were composed of LaB6 rich concentric belts surrounding large eutectic regions with a dense and uniform distribution of (TixZr1-x)B-2 fibers of 0.6 mu m in diameter inside a LaB6 matrix. The di- and hexa-boride mole fractions at eutectic points have been more accurately defined for x = 0-0.76. Fiber growth directions were modified by the addition of titanium. Diboride (subscript 2) fibers grew along [0 0 0 1](2) for x = 0 and along ((1) over bar 1 0 0)(2) for x not equal 0. The orientation of the hexaboride (subscript 6) matrix was unchanged with or without titanium addition. The favored crystallographic orientation relationship was: [0 0 1](6)//[0 0 0 1](2) and (1 1 0)(6)//(1 1 (2) over bar 0)(2) and ((1) over bar 1 0)(6)//((1) over bar 1 0 0)(2) for any x value. The dominant interfaces were {1 1 0}(6)//{1 1 (2) over bar 0}(2) for x = 0 and (0 0 1)(6)//(0 0 0 1)(2) for x not equal 0, the latter being expected to be energetically more favorable, as predicted by a 2D geometrical model. (C) 2014 Elsevier Ltd. All rights reserved.
C1 [Jouanny, I.; Sennour, M.; Berger, M. H.] MINES ParisTech, Ctr Mat, UMR CNRS 7633, F-91003 Evry, France.
[Filipov, V. B.; Ievdokyrnova, A.; Paderno, V. N.] Natl Acad Sci Ukraine, Frantsevitch Inst Problems Mat Sci, Kiev, Ukraine.
[Sayir, A.] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA.
RP Berger, MH (reprint author), MINES ParisTech, Ctr Mat, BP 87, F-91003 Evry, France.
EM marie-helene.berger@mines-paristech.fr
RI Berger, Marie-Helene/B-9785-2013
FU Air Force Office of Scientific Research [FA9550-09-1-0312]
FX Supported by the Air Force Office of Scientific Research under grant
AFOSR No. FA9550-09-1-0312.
NR 19
TC 0
Z9 0
U1 3
U2 20
PU ELSEVIER SCI LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND
SN 0955-2219
EI 1873-619X
J9 J EUR CERAM SOC
JI J. Eur. Ceram. Soc.
PD AUG
PY 2014
VL 34
IS 9
SI SI
BP 2101
EP 2109
DI 10.1016/j.jeurceramsoc.2014.01.026
PG 9
WC Materials Science, Ceramics
SC Materials Science
GA AH1HZ
UT WOS:000335872500009
ER
PT J
AU Tanner, A
Gaier, T
Imbriale, W
Kangaslahti, P
Lambrigtsen, B
Lim, B
AF Tanner, Alan
Gaier, Todd
Imbriale, William
Kangaslahti, Pekka
Lambrigtsen, Bjorn
Lim, Boon
TI A Dual-Gain Design for the Geostationary Synthetic Thinned Array
Radiometer
SO IEEE GEOSCIENCE AND REMOTE SENSING LETTERS
LA English
DT Article
DE Aperture synthesis; interferometer array; microwave radiometer
ID GEOSTAR DEMONSTRATOR INSTRUMENT
AB Anew geometry for synthetic aperture radiometers is presented which increases the distance between adjacent elements in the array without changing the visibility sample density in the u-v plane. This provides room for higher elemental antenna gain, which improves both the overall system sensitivity and alias rejection in the synthesized image-both critical requirements for the Earth observing application. The geometry is derived from the simple Y-array geometry by shifting alternate elements within an otherwise linear array arm into two or more rows of antennas. The resulting system largely retains the same hexagonal sample grid in the u-v plane of the visibility function, yet allows for an elemental antenna aperture that is physically larger than the u-v sample spacing. Only the shortest visibility baselines are lost, and a small dedicated low-gain array must be added to the system to recover these baselines. The radiometer is thus divided between a large high-gain array and a small low-gain array. Since the sensitivity (delta-T) of the system is dominated by that of the large array, this approach greatly improves the overall system sensitivity-in this letter, by a factor of 9 (or, equivalently, factor 81 integration time).
C1 [Tanner, Alan; Gaier, Todd; Imbriale, William; Kangaslahti, Pekka; Lambrigtsen, Bjorn; Lim, Boon] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Tanner, A (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
NR 9
TC 2
Z9 2
U1 0
U2 10
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 1545-598X
EI 1558-0571
J9 IEEE GEOSCI REMOTE S
JI IEEE Geosci. Remote Sens. Lett.
PD AUG
PY 2014
VL 11
IS 8
BP 1340
EP 1344
DI 10.1109/LGRS.2013.2293318
PG 5
WC Geochemistry & Geophysics; Engineering, Electrical & Electronic; Remote
Sensing; Imaging Science & Photographic Technology
SC Geochemistry & Geophysics; Engineering; Remote Sensing; Imaging Science
& Photographic Technology
GA AD2VY
UT WOS:000333095200006
ER
PT J
AU Le Vine, DM
de Matthaeis, P
Ruf, CS
AF Le Vine, David M.
de Matthaeis, Paolo
Ruf, Christopher S.
TI Aquarius RFI Detection and Mitigation Algorithm: Assessment and Examples
SO IEEE TRANSACTIONS ON GEOSCIENCE AND REMOTE SENSING
LA English
DT Article
DE Interference; microwave radiometry; remote sensing
ID L-BAND; SURFACE SALINITY; RADIOMETER; SPACE
AB Aquarius is an L-band radiometer system designed to map sea surface salinity from space. This is a sensitive measurement, and protection from radio frequency interference (RFI) is important for success. An initial look at the performance of the Aquarius RFI detection and mitigation algorithm is reported together with examples of the global distribution of RFI at the L-band. To protect against RFI, Aquarius employs rapid sampling (10 ms) and a "glitch" detection algorithm that looks for outliers among the samples. Samples identified as RFI are removed, and the remainder is averaged to produce an RFI-free signal for the salinity retrieval algorithm. The RFI detection algorithm appears to work well over the ocean with modest rates for false alarms (5%) and missed detection. The global distribution of RFI coincides well with population centers and is consistent with observations reported by the Soil Moisture and Ocean Salinity mission.
C1 [Le Vine, David M.; de Matthaeis, Paolo] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Ruf, Christopher S.] Univ Michigan, Ann Arbor, MI 48109 USA.
RP Le Vine, DM (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RI Ruf, Christopher/I-9463-2012
NR 21
TC 15
Z9 15
U1 2
U2 27
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 AUG
PY 2014
VL 52
IS 8
BP 4574
EP 4584
DI 10.1109/TGRS.2013.2282595
PG 11
WC Geochemistry & Geophysics; Engineering, Electrical & Electronic; Remote
Sensing; Imaging Science & Photographic Technology
SC Geochemistry & Geophysics; Engineering; Remote Sensing; Imaging Science
& Photographic Technology
GA AC5ZC
UT WOS:000332598500008
ER
PT J
AU Friedline, AW
Zachariah, MM
Johnson, K
Thomas, KJ
Middaugh, AN
Garimella, R
Powell, DR
Vaishampayan, PA
Rice, CV
AF Friedline, Anthony W.
Zachariah, Malcolm M.
Johnson, Karen
Thomas, Kieth J., III
Middaugh, Amy N.
Garimella, Ravindranath
Powell, Douglas R.
Vaishampayan, Parag A.
Rice, Charles V.
TI Water Behavior in Bacterial Spores by Deuterium NMR Spectroscopy
SO JOURNAL OF PHYSICAL CHEMISTRY B
LA English
DT Article
ID BACILLUS-SUBTILIS SPORES; CALCIUM DIPICOLINATE TRIHYDRATE;
NUCLEAR-MAGNETIC-RESONANCE; ACID-SOLUBLE PROTEINS; SOLAR UV-RADIATION;
SOLID-STATE NMR; H-2 NMR; HEAT-RESISTANCE; CA2+-DIPICOLINIC ACID;
DYNAMIC STRUCTURE
AB Dormant bacterial spores are able to survive long periods of time without nutrients, withstand harsh environmental conditions, and germinate into metabolically active bacteria when conditions are favorable. Numerous factors influence this hardiness, including the spore structure and the presence of compounds to protect DNA from damage. It is known that the water content of the spore core plays a role in resistance to degradation, but the exact state of water inside the core is a subject of discussion. Two main theories present themselves: either the water in the spore core is mostly immobile and the core and its components are in a glassy state, or the core is a gel with mobile water around components which themselves have limited mobility. Using deuterium solid-state NMR experiments, we examine the nature of the water in the spore core. Our data show the presence of unbound water, bound water, and deuterated biomolecules that also contain labile deuterons. Deuterium-hydrogen exchange experiments show that most of these deuterons are inaccessible by external water. We believe that these unreachable deuterons are in a chemical bonding state that prevents exchange. Variable-temperature NMR results suggest that the spore core is more rigid than would be expected for a gel-like state. However, our rigid core interpretation may only apply to dried spores whereas a gel core may exist in aqueous suspension. Nonetheless, the gel core, if present, is inaccessible to external water.
C1 [Friedline, Anthony W.; Zachariah, Malcolm M.; Johnson, Karen; Thomas, Kieth J., III; Middaugh, Amy N.; Garimella, Ravindranath; Powell, Douglas R.; Rice, Charles V.] Univ Oklahoma, Dept Chem & Biochem, Stephenson Life Sci Res Ctr, Norman, OK 73019 USA.
[Vaishampayan, Parag A.] CALTECH, Jet Prop Lab, Biotechnol & Planetary Protect Grp, Pasadena, CA 91109 USA.
RP Rice, CV (reprint author), Univ Oklahoma, Dept Chem & Biochem, Stephenson Life Sci Res Ctr, 101 Stephenson Pkwy, Norman, OK 73019 USA.
EM rice@ou.edu
FU National Institutes of Health [1R01GM090064-01]; NASA EPSCoR Research
Infrastructure Development (RID) grant [NN07AL49A]; University of
Oklahoma
FX This work is supported by the National Institutes of Health
(1R01GM090064-01), a NASA EPSCoR Research Infrastructure Development
(RID) grant (NN07AL49A), and the University of Oklahoma. We also wish to
express our gratitude to Dr. Kasthuri Venkateswaran, California
Institute of Technology, Jet Propulsion Laboratory, NASA, for insights
and helpful discussions.
NR 59
TC 5
Z9 5
U1 3
U2 12
PU AMER CHEMICAL SOC
PI WASHINGTON
PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA
SN 1520-6106
J9 J PHYS CHEM B
JI J. Phys. Chem. B
PD JUL 31
PY 2014
VL 118
IS 30
BP 8945
EP 8955
DI 10.1021/jp5025119
PG 11
WC Chemistry, Physical
SC Chemistry
GA AM5VX
UT WOS:000339930200004
PM 24950158
ER
PT J
AU Jensen, ELN
Akeson, R
AF Jensen, Eric L. N.
Akeson, Rachel
TI Misaligned protoplanetary disks in a young binary star system
SO NATURE
LA English
DT Article
ID ON CIRCUMSTELLAR DISK; T-TAURI STARS; PLANETARY ORBITS; ACCRETION DISCS;
TRIPLE SYSTEM; V4046 SGR; MU-M; EVOLUTION; PERTURBATIONS; OBLIQUITIES
AB Many extrasolar planets follow orbits that differ from the nearly coplanar and circular orbits found in our Solar System; their orbits may be eccentric(1) or inclined with respect to the host star's equator(2,3), and the population of giant planets orbiting close to their host stars suggests appreciable orbital migration(4). There is at present no consensus on what produces such orbits. Theoretical explanations often invoke interactions with a binary companion star in an orbit that is inclined relative to the planet's orbital plane(4,5). Such mechanisms require significant mutual inclinations between the planetary and binary star orbital planes. The protoplanetary disks in a few young binaries are misaligned(6-12), but often the measurements of these mis-alignments are sensitive only to a small portion of the inner disk, and the three-dimensional misalignment of the bulk of the planet-forming disk mass has hitherto not been determined. Here we report that the protoplanetary disks in the young binary system HK Tauri are misaligned by 60 to 68 degrees, such that one or both of the disks are significantly inclined to the binary orbital plane. Our results demonstrate that the necessary conditions exist for misalignment-driven mechanisms to modify planetary orbits, and that these conditions are present at the time of planet formation, apparently because of the binary formation process.
C1 [Jensen, Eric L. N.] Swarthmore Coll, Dept Phys & Astron, Swarthmore, PA 19081 USA.
[Akeson, Rachel] CALTECH, IPAC, NASA, Exoplanet Sci Inst, Pasadena, CA 91125 USA.
RP Jensen, ELN (reprint author), Swarthmore Coll, Dept Phys & Astron, 500 Coll Ave, Swarthmore, PA 19081 USA.
EM ejensen1@swarthmore.edu
OI Jensen, Eric/0000-0002-4625-7333
NR 47
TC 28
Z9 28
U1 2
U2 6
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 JUL 30
PY 2014
VL 511
IS 7511
BP 567
EP +
DI 10.1038/nature13521
PG 6
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA AM0VT
UT WOS:000339566300029
PM 25079553
ER
PT J
AU Molotch, NP
Meromy, L
AF Molotch, Noah P.
Meromy, Leah
TI Physiographic and climatic controls on snow cover persistence in the
Sierra Nevada Mountains
SO HYDROLOGICAL PROCESSES
LA English
DT Article; Proceedings Paper
CT Eastern Snow Conference (ESC)
CY JUN 04-06, 2013
CL Huntsville, CANADA
DE snow hydrology; remote sensing; water resources
ID WESTERN UNITED-STATES; RIO-GRANDE HEADWATERS; TELEMETRY SNOTEL DATA;
SUB-ALPINE FOREST; WATER EQUIVALENT; SPATIAL-DISTRIBUTION; THEMATIC
MAPPER; GRAIN-SIZE; MODEL; VARIABILITY
AB The persistence of snow cover across mountainous landscapes influences land-atmosphere energy exchange, water availability, the partitioning of snowmelt into various hydrologic pathways, vegetation productivity, and fluxes of nutrients. Understanding the processes controlling snow cover persistence has been limited as relationships between physiography, climate, and snow persistence are nonlinear and difficult to characterize empirically. The work detailed herein uses 7 years of remotely sensed snow cover persistence observed from the Moderate Resolution Imaging Spectroradiometer over the Sierra Nevada Mountains as a dependent variable in binary regression tree models with a suite of independent variables comprised of both physiographic and climatic metrics. Annual snow cover persistence over 2001-2007 revealed significant inter-annual variability, with domain-average snow persistence values exceeding 4.01 (i. e. early April) in the wettest year of 2005 and reaching as low as 2.90 (i. e. late February) in the driest year of 2007. Regression tree models revealed that elevation was the most important explanatory variable regarding snow cover persistence, ranking first in the hierarchical models in 10 out of 13 watersheds. Precipitation (Feather and Owens River basins) and temperature (Kern River basin) were the first-ranking variables in the remaining three watersheds. Second, the order variables of importance included vegetation, which ranked between 2nd and 5th in 10 of 13 watersheds, and slope, which ranked 4th and 5th in 12 of the 13 watersheds. Interestingly, solar radiation and aspect were of tertiary importance but were more influential in watersheds with north-south orientation (e. g. in the Feather, Mokelumne and Stanislaus watersheds). These results have implications for understanding the sensitivity of snow cover persistence to changes in climate as watersheds where elevation and/or temperature strongly influence snow cover persistence may be more sensitive to future warming. Further work is needed to identify associated ecosystem sensitivities to future changes in snow cover persistence. Copyright (C) 2014 John Wiley & Sons, Ltd.
C1 [Molotch, Noah P.; Meromy, Leah] Univ Colorado, Inst Arctic & Alpine Res, Dept Geog, Boulder, CO 80303 USA.
[Molotch, Noah P.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Molotch, NP (reprint author), Univ Colorado, Inst Arctic & Alpine Res, Dept Geog, Boulder, CO 80303 USA.
EM Noah.Molotch@colorado.edu
RI Zhang, Jianming/A-2994-2011; Molotch, Noah/C-8576-2009
OI Zhang, Jianming/0000-0001-7053-7696;
FU NASA [NNX08AH18G, NNX11AK35A, NNX11AK35G, NNX10AO97G]; NSF [EAR 1032295,
EAR 1141764]; USDA [2012-67003-19802]; NOAA RISA Western Water
Assessment fund; United States American Recovery and Reinvestment Act
fund
FX This research was supported by NASA grants NNX08AH18G, NNX11AK35A,
NNX11AK35G and NNX10AO97G, NSF grants EAR 1032295 and EAR 1141764, USDA
grant 2012-67003-19802, the NOAA RISA Western Water Assessment and
United States American Recovery and Reinvestment Act funds. Part of
NPM's contributions for this study was carried out on behalf of the Jet
Propulsion Laboratory, California Institute of Technology, under a
contract with the National Aeronautics and Space Administration.
NR 86
TC 2
Z9 2
U1 3
U2 40
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 0885-6087
EI 1099-1085
J9 HYDROL PROCESS
JI Hydrol. Process.
PD JUL 30
PY 2014
VL 28
IS 16
SI SI
BP 4573
EP 4586
DI 10.1002/hyp.10254
PG 14
WC Water Resources
SC Water Resources
GA AM2YO
UT WOS:000339717800004
ER
PT J
AU Sugg, JW
Perry, LB
Hall, DK
Riggs, GA
Badurek, CA
AF Sugg, Johnathan W.
Perry, L. Baker
Hall, Dorothy K.
Riggs, George A.
Badurek, Christopher A.
TI Satellite perspectives on the spatial patterns of new snowfall in the
Southern Appalachian Mountains
SO HYDROLOGICAL PROCESSES
LA English
DT Article; Proceedings Paper
CT Eastern Snow Conference (ESC)
CY JUN 04-06, 2013
CL Huntsville, CANADA
DE fractional snow cover; MODIS; synoptic-scale circulation; Southern
Appalachian Mountains
ID FLOW SNOWFALL; NEW-ZEALAND; MODIS; COVER; ALBEDO; PRECIPITATION; TURKEY;
PRODUCTS; TERRAIN; FORESTS
AB The Southern Appalachian Mountains (SAM) are a heavily forested mid-latitude mountain region that provide an ideal location for assessing the suitability of satellite-derived snow maps and explicitly linking atmospheric circulation to the spatial patterns of new snowfall. Although a variety of synoptic-scale circulation regimes contribute to mean annual snowfall, which ranges from roughly 25 cm in the lowest valleys to over 250 cm at the highest elevations, atmospheric circulation processes have largely been absent from efforts seeking to quantify the spatial patterns of new snowfall. In this paper, we examine the suitability of fractional snow cover (FSC) maps from the Moderate Resolution Imaging Spectroradiometer (MODIS) and determine the spatial extent of snowfall according to synoptic-scale circulation. FSC maps are analysed after 122 snow events from 2006 to 2012 to provide a suitability analysis of MODIS products for use in the SAM. For each event, we calculate FSC distribution and total snow-covered area and compare it with available in situ observations. Results indicate that the SAM presents unique meteorological, physical, and spectral characteristics that are ideal for evaluating the suitability of MODIS for measuring snow cover. Out of 122 observed snow events, 63 are considered suitable for analysis with the FSC maps. The highest FSC values are observed after Gulf/Atlantic lows and south-eastward tracking clipper systems. We conclude that MODIS data can be successfully used to link broader atmospheric circulation processes of snowfall with the spatial patterns of snow cover. Copyright (C) 2014 John Wiley & Sons, Ltd.
C1 [Sugg, Johnathan W.] Univ N Carolina, Dept Geog, Chapel Hill, NC 27599 USA.
[Perry, L. Baker; Badurek, Christopher A.] Appalachian State Univ, Dept Geog & Planning, Boone, NC 28608 USA.
[Hall, Dorothy K.; Riggs, George A.] NASA, Goddard Space Flight Ctr, Cryospher Sci Lab, Greenbelt, MD 20771 USA.
[Riggs, George A.] Sci Syst & Applicat Inc, Lanham, MD USA.
RP Sugg, JW (reprint author), Univ N Carolina, Dept Geog, Chapel Hill, NC 27599 USA.
EM jwsugg@live.unc.edu
RI Badurek, Christopher/A-8114-2015
OI Badurek, Christopher/0000-0001-5741-4333
FU North Carolina Space Grant; Appalachian State University Department of
Geography and Planning; Office of Student Research; Cratis D. Williams
Graduate School
FX The authors thank the following data sources: the NASA's REVERB ECHO
Data Portal, the NWS COOP network, National Oceanic and Atmospheric
Administration's Hydrometeorological Prediction Center, the State
Climate Office of North Carolina, and the University of
Wisconsin-Madison Space Science and Engineering Center. Funding support
was provided by the North Carolina Space Grant, Appalachian State
University Department of Geography and Planning, Office of Student
Research, and the Cratis D. Williams Graduate School. The authors
declare no conflict of interest.
NR 37
TC 1
Z9 1
U1 2
U2 3
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 0885-6087
EI 1099-1085
J9 HYDROL PROCESS
JI Hydrol. Process.
PD JUL 30
PY 2014
VL 28
IS 16
SI SI
BP 4602
EP 4613
DI 10.1002/hyp.10196
PG 12
WC Water Resources
SC Water Resources
GA AM2YO
UT WOS:000339717800006
ER
PT J
AU Parker, ET
Zhou, MS
Burton, AS
Glavin, DP
Dworkin, JP
Krishnamurthy, R
Fernandez, FM
Bada, JL
AF Parker, Eric T.
Zhou, Manshui
Burton, Aaron S.
Glavin, Daniel P.
Dworkin, Jason P.
Krishnamurthy, Ramanarayanan
Fernandez, Facundo M.
Bada, Jeffrey L.
TI A Plausible Simultaneous Synthesis of Amino Acids and Simple Peptides on
the Primordial Earth
SO ANGEWANDTE CHEMIE-INTERNATIONAL EDITION
LA English
DT Article
DE amino acids; cyanamide; mass spectrometry; peptides; polymerization
ID SPARK DISCHARGE EXPERIMENT; PREBIOTIC CHEMISTRY; MURCHISON METEORITE;
HYDROLYSIS; EVOLUTION; CYANAMIDE; ATMOSPHERE; OCEAN
AB Following his seminal work in 1953, Stanley Miller conducted an experiment in 1958 to study the polymerization of amino acids under simulated early Earth conditions. In the experiment, Miller sparked a gas mixture of CH4, NH3, and H2O, while intermittently adding the plausible prebiotic condensing reagent cyanamide. For unknown reasons, an analysis of the samples was not reported. We analyzed the archived samples for amino acids, dipeptides, and diketopiperazines by liquid chromatography, ion mobility spectrometry, and mass spectrometry. A dozen amino acids, 10 glycine-containing dipeptides, and 3 glycine-containing diketopiperazines were detected. Miller's experiment was repeated and similar polymerization products were observed. Aqueous heating experiments indicate that Strecker synthesis intermediates play a key role in facilitating polymerization. These results highlight the potential importance of condensing reagents in generating diversity within the prebiotic chemical inventory.
C1 [Parker, Eric T.; Zhou, Manshui; Fernandez, Facundo M.] Georgia Inst Technol, Sch Chem & Biochem, Atlanta, GA 30332 USA.
[Burton, Aaron S.] NASA, Astromat Res & Explorat Sci Directorate, Johnson Space Ctr, Houston, TX 77058 USA.
[Glavin, Daniel P.; Dworkin, Jason P.] NASA, Goddard Space Flight Ctr, Solar Syst Explorat Div, Greenbelt, MD 20771 USA.
[Krishnamurthy, Ramanarayanan] Scripps Res Inst, Dept Chem, La Jolla, CA 92037 USA.
[Bada, Jeffrey L.] Univ Calif San Diego, Scripps Inst Oceanog, Geophys Res Div, La Jolla, CA 92093 USA.
RP Fernandez, FM (reprint author), Georgia Inst Technol, Sch Chem & Biochem, 901 Atlantic Dr NW, Atlanta, GA 30332 USA.
EM facundo.fernandez@chemistry.gatech.edu; jbada@ucsd.edu
RI Burton, Aaron/H-2212-2011; 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; Krishnamurthy,
Ramanarayanan/0000-0001-5238-610X
FU Center for Chemical Evolution at the Georgia Institute of Technology by
NSF [CHE-1004570]; Center for Chemical Evolution at the Georgia
Institute of Technology by NASA Astrobiology Program (NSF) [CHE-100457];
Marine Biology Laboratory's NASA Planetary Biology Internship Program;
NASA Postdoctoral Program at the Goddard Space Flight Center; NASA
FX This research was supported by the Center for Chemical Evolution at the
Georgia Institute of Technology, jointly supported by the NSF and the
NASA Astrobiology Program (NSF CHE-1004570). E.T.P. acknowledges
financial support from the Marine Biology Laboratory's NASA Planetary
Biology Internship Program. A.S.B. acknowledges support from the NASA
Postdoctoral Program at the Goddard Space Flight Center, administered by
Oak Ridge Associated Universities through a contract with NASA. J.P.D.
and D.P.G. acknowledge the Goddard Center for Astrobiology and the NASA
Astrobiology Institute. We are appreciative of the Mandeville Special
Collections at the Geisel Library on the campus of the University of
California, San Diego for archiving Miller's original laboratory
notebooks and providing assistance with retrieving them.
NR 42
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U1 8
U2 75
PU WILEY-V C H VERLAG GMBH
PI WEINHEIM
PA BOSCHSTRASSE 12, D-69469 WEINHEIM, GERMANY
SN 1433-7851
EI 1521-3773
J9 ANGEW CHEM INT EDIT
JI Angew. Chem.-Int. Edit.
PD JUL 28
PY 2014
VL 53
IS 31
BP 8132
EP 8136
DI 10.1002/anie.201403683
PG 5
WC Chemistry, Multidisciplinary
SC Chemistry
GA AN3WZ
UT WOS:000340520700026
PM 24966137
ER
PT J
AU Gronoff, G
Rahmati, A
SimonWedlund, C
Mertens, CJ
Cravens, TE
Kallio, E
AF Gronoff, Guillaume
Rahmati, Ali
SimonWedlund, Cyril
Mertens, Christopher J.
Cravens, Thomas E.
Kallio, Esa
TI The precipitation of keV energetic oxygen ions at Mars and their effects
during the comet Siding Spring approach
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
ID LYMAN-ALPHA OBSERVATIONS; C/2013 A1; PICKUP IONS; C/1996 B2; IONOSPHERE;
HYAKUTAKE; DEGRADATION; ATMOSPHERE; SPACECRAFT; TRANSPORT
AB Comet Siding Spring C/2013 A1 will pass Mars on 19 October 2014, entailing particle and dust precipitation in the Martian upper atmosphere and a potential dust hazard for orbiters. An estimate of the flux of energetic O+ ions picked up by the solar wind from the cometary coma is shown, with an increase of the O+ flux above 50 keV by 2 orders of magnitude. While the ionization of Mars' upper atmosphere by precipitating O+ ions is expected to be negligible compared to solar EUV-XUV ionization, it is of the same order of magnitude at 110 km altitude during the cometary passage, leading to detectable increases in ionospheric densities. Cometary O+ pickup ion precipitation is expected to be the major nightside ionization source, creating a temporary ionosphere and a global airglow. These effects are dependent on the solar and cometary activities at the time of the encounter.
C1 [Gronoff, Guillaume; Mertens, Christopher J.] NASA Langley Res Ctr, Sci Directorate, Chem & Dynam Branch, Hampton, VA 23681 USA.
[Gronoff, Guillaume] SSAI, Hampton, VA USA.
[Rahmati, Ali; Cravens, Thomas E.] Univ Kansas, Dept Phys & Astron, Lawrence, KS 66045 USA.
[SimonWedlund, Cyril; Kallio, Esa] Aalto Univ, Sch Elect Engn, Dept Radio Sci & Engn, Aalto, Finland.
RP Gronoff, G (reprint author), NASA Langley Res Ctr, Sci Directorate, Chem & Dynam Branch, Hampton, VA 23681 USA.
EM Guillaume.P.Gronoff@nasa.gov
RI Kallio, Esa/F-9410-2014;
OI Kallio, Esa/0000-0002-9791-804X; Gronoff, Guillaume/0000-0002-0331-7076
NR 49
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Z9 9
U1 0
U2 4
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 JUL 28
PY 2014
VL 41
IS 14
BP 4844
EP 4850
DI 10.1002/2014GL060902
PG 7
WC Geosciences, Multidisciplinary
SC Geology
GA AN4CU
UT WOS:000340536000006
ER
PT J
AU Poppe, AR
Sarantos, M
Halekas, JS
Delory, GT
Saito, Y
Nishino, M
AF Poppe, A. R.
Sarantos, M.
Halekas, J. S.
Delory, G. T.
Saito, Y.
Nishino, M.
TI Anisotropic solar wind sputtering of the lunar surface induced by
crustal magnetic anomalies
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
ID FIELDS; EXOSPHERE; REGOLITH; ATOMS
AB The lunar exosphere is generated by several processes each of which generates neutral distributions with different spatial and temporal variability. Solar wind sputtering of the lunar surface is a major process for many regolith-derived species and typically generates neutral distributions with a cosine dependence on solar zenith angle. Complicating this picture are remanent crustal magnetic anomalies on the lunar surface, which decelerate and partially reflect the solar wind before it strikes the surface. We use Kaguya maps of solar wind reflection efficiencies, Lunar Prospector maps of crustal field strengths, and published neutral sputtering yields to calculate anisotropic solar wind sputtering maps. We feed these maps to a Monte Carlo neutral exospheric model to explore three-dimensional exospheric anisotropies and find that significant anisotropies should be present in the neutral exosphere depending on selenographic location and solar wind conditions. Better understanding of solar wind/crustal anomaly interactions could potentially improve our results.
C1 [Poppe, A. R.; Halekas, J. S.; Delory, G. T.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
[Poppe, A. R.; Sarantos, M.; Halekas, J. S.; Delory, G. T.] NASA Ames Res Ctr, Solar Syst Explorat Res Virtual Inst, Mountain View, CA USA.
[Sarantos, M.] Univ Maryland Baltimore Cty, Goddard Planetary Heliophys Inst, Baltimore, MD 21228 USA.
[Sarantos, M.] NASA Goddard Space Flight Ctr, Greenbelt, MD USA.
[Saito, Y.] Japan Aerosp Explorat Agcy, Inst Space & Astronaut Sci, Tokyo, Japan.
[Nishino, M.] Nagoya Univ, Solar Terr Environm Lab, Nagoya, Aichi 4648601, Japan.
RP Poppe, AR (reprint author), Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
EM poppe@ssl.berkeley.edu
OI Poppe, Andrew/0000-0001-8137-8176; Halekas, Jasper/0000-0001-5258-6128
FU NASA's Lunar Atmospheric and Dust Environment Explorer (LADEE) Guest
Investigator program [NNX13AO71G, NNX13AO74G]; NASA's Solar System
Exploration Research Virtual Institute
FX The authors gratefully acknowledge support from NASA's Lunar Atmospheric
and Dust Environment Explorer (LADEE) Guest Investigator program, grants
NNX13AO71G (A. R. P. and J.S.H.) and NNX13AO74G (M. S.). The authors
also acknowledge support by NASA's Solar System Exploration Research
Virtual Institute. This publication is SSERVI contribution
SSERVI-2014-097. The Kaguya data used in this study are available upon
request to the authors, while the Lunar Prospector data can be found in
the NASA Planetary Data System (PDS).
NR 37
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U2 9
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 JUL 28
PY 2014
VL 41
IS 14
BP 4865
EP 4872
DI 10.1002/2014GL060523
PG 8
WC Geosciences, Multidisciplinary
SC Geology
GA AN4CU
UT WOS:000340536000009
ER
PT J
AU Schorghofer, N
AF Schorghofer, Norbert
TI Migration calculations for water in the exosphere of the Moon: Dusk-dawn
asymmetry, heterogeneous trapping, and D/H fractionation
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
ID LUNAR POLAR-REGIONS; SOLAR-WIND; PARENT MOLECULES; ICE; SURFACE; POLES;
VOLATILES; MERCURY
AB Water ice is trapped in permanently shadowed craters near the lunar poles, where it is thought to have arrived from an exogenic or endogenic source via ballistic hops. We use a model of the migration of water molecules in the lunar exosphere to investigate three problems: (1) A strong continuous source would lead to an enhanced concentration of H2O at the morning terminator but not at the evening terminator. Hence, spectral features observed at both terminators do not suggest that there is diurnal migration of volatiles. (2) Cold trapping after a comet impact leads to an unequal partitioning between the two hemispheres depending on the latitude of the impact but to nearly equal partitioning with respect to longitude. (3) The D/H fractionation as the water molecules migrate toward the poles is small. Hence, the isotopic composition of ice deposits in the cold traps can be related to that of the source.
C1 [Schorghofer, Norbert] Univ Hawaii Manoa, Inst Astron, Honolulu, HI 96822 USA.
[Schorghofer, Norbert] Univ Hawaii Manoa, NASA Astrobiol Inst, Honolulu, HI 96822 USA.
RP Schorghofer, N (reprint author), Univ Hawaii Manoa, Inst Astron, Honolulu, HI 96822 USA.
EM norbert@hawaii.edu
FU National Aeronautics and Space Administration through the NASA
Astrobiology Institute [NNA09DA77A]
FX This material is based upon work supported by the National Aeronautics
and Space Administration through the NASA Astrobiology Institute under
Cooperative agreement NNA09DA77A issued through the Office of Space
Science. The author is also grateful for the hospitality of the
International Space Science Institute (ISSI) in Bern and the Keck
Institute for Space Studies (KISS) at Caltech.
NR 28
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U1 1
U2 3
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 JUL 28
PY 2014
VL 41
IS 14
BP 4888
EP 4893
DI 10.1002/2014GL060820
PG 6
WC Geosciences, Multidisciplinary
SC Geology
GA AN4CU
UT WOS:000340536000012
ER
PT J
AU Qiu, JX
Crow, WT
Nearing, GS
Mo, XG
Liu, SX
AF Qiu, Jianxiu
Crow, Wade T.
Nearing, Grey S.
Mo, Xingguo
Liu, Suxia
TI The impact of vertical measurement depth on the information content of
soil moisture times series data
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
ID SEQUENTIAL ASSIMILATION; ERS SCATTEROMETER; NEAR-SURFACE; VALIDATION;
PRODUCTS; FILTER
AB Using a decade of ground-based soil moisture observations acquired from the United States Department of Agriculture's Soil Climate Analysis Network (SCAN), we calculate the mutual information (MI) content between multiple soil moisture variables and near-future vegetation condition to examine the existence of emergent drought information in vertically integrated (surface to 60 cm) soil moisture observations (theta(0-60) ([cm])) not present in either superficial soil moisture observations (theta(5) ([cm])) or a simple low-pass transformation of theta(5). Results suggest that while theta(0-60) is indeed more valuable than theta(5) for predicting near-future vegetation anomalies, the enhanced information content in theta(0-60) soil moisture can be effectively duplicated by the low-pass transformation of theta(5). This implies that, for drought monitoring applications, the shallow vertical penetration depth of microwave-based theta(5) retrievals does not represent as large a practical limitation as commonly perceived.
C1 [Qiu, Jianxiu; Mo, Xingguo; Liu, Suxia] Chinese Acad Sci, Inst Geog Sci & Nat Resources Res, Key Lab Water Cycle & Related Land Surface Proc, Beijing, Peoples R China.
[Qiu, Jianxiu; Crow, Wade T.] ARS, USDA, Hydrol & Remote Sensing Lab, Beltsville, MD 20705 USA.
[Nearing, Grey S.] NASA Goddard Space Flight Ctr, Hydrol Sci Lab, Greenbelt, MD USA.
RP Crow, WT (reprint author), ARS, USDA, Hydrol & Remote Sensing Lab, Beltsville, MD 20705 USA.
EM Wade.Crow@ars.usda.gov
RI Qiu, Jianxiu/O-6255-2016
OI Qiu, Jianxiu/0000-0002-1275-4171
FU Natural Science Foundation of China [31171451]; Key Project for the
Strategic Science Plan in IGSNRR, CAS [2012ZD003]; Chinese Scholarship
Council; NASA Terrestrial Ecology Program [NNH09ZDA001N]
FX The soil moisture data set for this paper is available at USDA SCAN
website (see http://www.wcc.nrcs.usda.gov/scan/), and MODIS surface
reflectance and land cover data are available at
http://modis.gsfc.nasa.gov. Thanks to the Natural Science Foundation of
China grant (31171451), the Key Project for the Strategic Science Plan
in IGSNRR, CAS (2012ZD003), and the Chinese Scholarship Council for
supporting the first author to conduct research at the USDA-ARS
Hydrology and Remote Sensing Laboratory. This work was also partially
supported by a grant from the NASA Terrestrial Ecology Program
(NNH09ZDA001N) to W. T. Crow.
NR 29
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U2 14
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 JUL 28
PY 2014
VL 41
IS 14
BP 4997
EP 5004
DI 10.1002/2014GL060017
PG 8
WC Geosciences, Multidisciplinary
SC Geology
GA AN4CU
UT WOS:000340536000025
ER
PT J
AU Kwok, R
AF Kwok, R.
TI Simulated effects of a snow layer on retrieval of CryoSat-2 sea ice
freeboard
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
AB The impact of a snow layer on the location of the tracking point (RP) for ranging to the sea ice surface in CryoSat-2 synthetic aperture interferometric radar altimeter waveforms is simulated. With a range resolution of similar to 47 cm, the response of the air-snow (a-s) interface broadens the response of the snow-ice (s-i) interface and displaces the RP toward the altimeter. This effect is largest when the strengths of their returns are comparable and when snow thicknesses are > 20 cm. On the other hand, the RP is displaced away from the altimeter when the reduced propagation speed in the snow layer is not accounted for. This analysis examines the dependence of these competing corrections on snow thickness and the relative scattering strengths of the interfaces and the sensitivity of two different tracking approaches (leading edge and centroid) to these snow parameters. Expected errors depend on a better understanding of the relative scattering strengths of the interfaces and snow layer.
C1 CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
RP Kwok, R (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
EM ron.kwok@jpl.nasa.gov
RI Kwok, Ron/A-9762-2008
OI Kwok, Ron/0000-0003-4051-5896
FU National Aeronautics and Space Administration
FX I thank Shirley Pang for the software support during the course of this
study. Data from Operation IceBridge are provided by the National Snow
and Ice Data Center. R. K. performed this work at the Jet Propulsion
Laboratory, California Institute of Technology, under contract with the
National Aeronautics and Space Administration.
NR 9
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U1 0
U2 9
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 JUL 28
PY 2014
VL 41
IS 14
BP 5014
EP 5020
DI 10.1002/2014GL060993
PG 7
WC Geosciences, Multidisciplinary
SC Geology
GA AN4CU
UT WOS:000340536000027
ER
PT J
AU Liang, Q
Newman, PA
Daniel, JS
Reimann, S
Hall, BD
Dutton, G
Kuijpers, LJM
AF Liang, Qing
Newman, Paul A.
Daniel, John S.
Reimann, Stefan
Hall, Bradley D.
Dutton, Geoff
Kuijpers, Lambert J. M.
TI Constraining the carbon tetrachloride (CCl4) budget using its global
trend and inter-hemispheric gradient
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
ID EMISSIONS; TRANSPORT; STRATOSPHERE; TROPOSPHERE; CHLORINE; FUTURE; GASES
AB Carbon tetrachloride (CCl4) is a major anthropogenic ozone-depleting substance and greenhouse gas and has been regulated under the Montreal Protocol. However, the near-zero 2007-2012 emissions estimate based on the UNEP reported production and feedstock usage cannot be reconciled with the observed slow decline of atmospheric concentrations and the inter-hemispheric gradient (IHG) for CCl4. Our 3-D model simulations suggest that the observed IHG (1.5 +/- 0.2 ppt for 2000-2012) is primarily caused by ongoing current emissions, while ocean and soil losses and stratosphere-troposphere exchange together contribute a small negative gradient (similar to 0 - -0.3 ppt). Using the observed CCl4 global trend and IHG, we deduce that the mean global emissions for the 2000-2012 period are 39(34)(45) Gg/yr (similar to 30% of the peak 1980s emissions) and a corresponding total lifetime of 35(37)(32) years.
C1 [Liang, Qing; Newman, Paul A.] NASA, Goddard Space Flight Ctr, Atmospher Chem & Dynam Lab, Greenbelt, MD 20771 USA.
[Liang, Qing] Univ Space Res Assoc, GESTAR, Columbia, MD USA.
[Daniel, John S.] NOAA, Earth Syst Res Lab, Div Chem Sci, Boulder, CO USA.
[Reimann, Stefan] Empa, Fed Labs Mat Sci & Technol, Dubendorf, Switzerland.
[Hall, Bradley D.; Dutton, Geoff] NOAA, Earth Syst Res Lab, Global Monitoring Div, Boulder, CO USA.
[Dutton, Geoff] Univ Colorado, Cooperat Inst Res Environm Sci, Boulder, CO 80309 USA.
[Kuijpers, Lambert J. M.] Tech Univ Eindhoven, NL-5600 MB Eindhoven, Netherlands.
RP Liang, Q (reprint author), NASA, Goddard Space Flight Ctr, Atmospher Chem & Dynam Lab, Greenbelt, MD 20771 USA.
EM Qing.Liang-1@nasa.gov
RI Liang, Qing/B-1276-2011; Daniel, John/D-9324-2011; Reimann,
Stefan/A-2327-2009; Manager, CSD Publications/B-2789-2015
OI Reimann, Stefan/0000-0002-9885-7138;
NR 30
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U1 1
U2 25
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 JUL 28
PY 2014
VL 41
IS 14
BP 5307
EP 5315
DI 10.1002/2014GL060754
PG 9
WC Geosciences, Multidisciplinary
SC Geology
GA AN4CU
UT WOS:000340536000052
ER
PT J
AU Carlson, AE
Hoffmayer, ER
Tribuzio, CA
Sulikowski, JA
AF Carlson, Amy E.
Hoffmayer, Eric R.
Tribuzio, Cindy A.
Sulikowski, James A.
TI The Use of Satellite Tags to Redefine Movement Patterns of Spiny Dogfish
(Squalus acanthias) along the US East Coast: Implications for Fisheries
Management
SO PLOS ONE
LA English
DT Article
ID ATLANTIC BLUEFIN TUNA; SEA-SURFACE TEMPERATURE; SHARKS
CARCHARODON-CARCHARIAS; DIEL VERTICAL MIGRATION; LIGHT-BASED
GEOLOCATION; OFFSHORE FORAGING AREA; BOTTOM-TRAWL SURVEY; STATE-SPACE
MODEL; GULF-OF-MEXICO; PACIFIC-OCEAN
AB Spiny dogfish (Squalus acanthias) are assumed to be a highly migratory species, making habitual north-south migrations throughout their northwestern Atlantic United States (U.S.) range. Also assumed to be a benthic species, spiny dogfish stock structure is estimated through Northeast Fisheries Science Center (NEFSC) bottom-trawl surveys. Recent anomalies in population trends, including a recent four-fold increase in estimated spawning stock biomass, suggest alternative movement patterns could exist for this shark species. To obtain a better understanding of the horizontal and vertical movement dynamics of this species, Microwave Telemetry pop-up satellite archival X-Tags were attached to forty adult spiny dogfish at the northern (Gulf of Maine) and southern (North Carolina) extents of their core U.S. geographic range. Reconstructed geolocation tracks ranging in lengths from two to 12 months suggest that the seasonal migration patterns appear to be local in nature to each respective northern and southern deployment site, differing from previously published migration paradigms. Differences in distance and direction traveled between seasonal geolocations possibly indicate separate migratory patterns between groups. Kernel utilization distribution models also suggest strong separate core home ranges. Significant differences in seasonal temperature and depths between the two regions further substantiate the possibility of separate regional movement patterns between the two groups. Vertical utilization also suggests distinct diel patterns and that this species may not utilize the benthos as previously thought, potentially decreasing availability to benthic gear.
C1 [Carlson, Amy E.; Sulikowski, James A.] Univ New England, Ctr Marine Sci, Biddeford, ME 04005 USA.
[Hoffmayer, Eric R.] Southeast Fisheries Sci Ctr, Mississippi Labs, Natl Marine Fisheries Serv, Pascagoula, MS USA.
[Tribuzio, Cindy A.] Alaska Fisheries Sci Ctr, Auke Bay Labs, Natl Marine Fisheries Serv, Juneau, AK USA.
RP Carlson, AE (reprint author), Univ New England, Ctr Marine Sci, Biddeford, ME 04005 USA.
EM acarlson1@une.edu
FU Saltonstall-Kennedy (S-K) Grant Program [NA09NMF4270099,
NA10NMF4270203]; Sturdivant Island Tuna Association
FX This project was supported by awards from the Saltonstall-Kennedy (S-K)
Grant Program (NA09NMF4270099 and NA10NMF4270203) and Sturdivant Island
Tuna Association to J.A.S. The funders had no role in study design, data
collection and analysis, decision to publish, or preparation of the
manuscript.
NR 112
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U1 6
U2 47
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 JUL 28
PY 2014
VL 9
IS 7
AR e103384
DI 10.1371/journal.pone.0103384
PG 16
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA AM6RZ
UT WOS:000339993700066
PM 25068584
ER
PT J
AU McConnell, JR
Maselli, OJ
Sigl, M
Vallelonga, P
Neumann, T
Anschutz, H
Bales, RC
Curran, MAJ
Das, SB
Edwards, R
Kipfstuhl, S
Layman, L
Thomas, ER
AF McConnell, J. R.
Maselli, O. J.
Sigl, M.
Vallelonga, P.
Neumann, T.
Anschutz, H.
Bales, R. C.
Curran, M. A. J.
Das, S. B.
Edwards, R.
Kipfstuhl, S.
Layman, L.
Thomas, E. R.
TI Antarctic-wide array of high-resolution ice core records reveals
pervasive lead pollution began in 1889 and persists today
SO SCIENTIFIC REPORTS
LA English
DT Article
ID COATS LAND; LAW DOME; SNOW; GREENLAND; AD; ISOTOPES; CLIMATE
AB Interior Antarctica is among the most remote places on Earth and was thought to be beyond the reach of human impacts when Amundsen and Scott raced to the South Pole in 1911. Here we show detailed measurements from an extensive array of 16 ice cores quantifying substantial toxic heavy metal lead pollution at South Pole and throughout Antarctica by 1889 - beating polar explorers by more than 22 years. Unlike the Arctic where lead pollution peaked in the 1970s, lead pollution in Antarctica was as high in the early 20th century as at any time since industrialization. The similar timing and magnitude of changes in lead deposition across Antarctica, as well as the characteristic isotopic signature of Broken Hill lead found throughout the continent, suggest that this single emission source in southern Australia was responsible for the introduction of lead pollution into Antarctica at the end of the 19th century and remains a significant source today. An estimated 660 t of industrial lead have been deposited over Antarctica during the past 130 years as a result of mid-latitude industrial emissions, with regional-to-global scale circulation likely modulating aerosol concentrations. Despite abatement efforts, significant lead pollution in Antarctica persists into the 21st century.
C1 [McConnell, J. R.; Maselli, O. J.; Sigl, M.; Layman, L.] Desert Res Inst, Reno, NV 89512 USA.
[Vallelonga, P.] Univ Copenhagen, Ctr Ice & Climate, DK-1168 Copenhagen, Denmark.
[Neumann, T.] NASA, Goddard Space Flight Ctr, Greenbelt, MD USA.
[Anschutz, H.] Norwegian Geotech Inst, Oslo, Norway.
[Bales, R. C.] Univ Calif, Merced, CA USA.
[Curran, M. A. J.] Australian Antarctic Div, Kingston, Tas, Australia.
[Das, S. B.] Woods Hole Oceanog Inst, Woods Hole, MA USA.
[Edwards, R.] Curtin Univ, Perth, WA, Australia.
[Kipfstuhl, S.] Helmholtz Zentrum Polar & Meeresforsch, Alfred Wegener Inst, Bremerhaven, Germany.
[Thomas, E. R.] British Antarctic Survey, Cambridge, England.
RP McConnell, JR (reprint author), Desert Res Inst, Reno, NV 89512 USA.
EM Joe.McConnell@dri.edu
RI Maselli, Olivia/A-6687-2013; Neumann, Thomas/D-5264-2012; Vallelonga,
Paul/I-9650-2016; Edwards, Ross/B-1433-2013
OI Vallelonga, Paul/0000-0003-1055-7235; Edwards, Ross/0000-0002-9233-8775
FU U. S. National Science Foundation Division of Polar Programs [9903744,
0538427, 0538416, 0968391, 1142166, 0632031]; instrument grants
[0216552, 0421412]; national research programs
FX The data reported in this paper are tabulated in the Supplementary
Information. This work primarily was supported by the U. S. National
Science Foundation Division of Polar Programs (research grants 9903744,
0538427, 0538416, 0968391, 1142166, 0632031; instrument grants 0216552,
0421412). We gratefully acknowledge the national research programs for
their support and the efforts of field teams and others for help in
collecting the ice cores in the array. The authors also thank the WAIS
Divide Science Coordination Office for the collection and distribution
of the WAIS Divide ice cores, Ice Drilling and Design and Operations for
drilling support, the National Ice Core Laboratory for curating many of
the cores used in this study; Raytheon Polar Service for logistics
support in Antarctica; and the 109th New York Air National Guard for
airlift in Antarctic.
NR 32
TC 13
Z9 13
U1 5
U2 39
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 JUL 28
PY 2014
VL 4
AR 5848
DI 10.1038/srep05848
PG 5
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA AM0CT
UT WOS:000339511300001
PM 25068819
ER
PT J
AU Goldstein, ME
AF Goldstein, M. E.
TI Effect of free-stream turbulence on boundary layer transition
SO PHILOSOPHICAL TRANSACTIONS OF THE ROYAL SOCIETY A-MATHEMATICAL PHYSICAL
AND ENGINEERING SCIENCES
LA English
DT Review
DE boundary layer transition; free-stream turbulence; boundary layer
streaks
ID VORTICAL DISTURBANCES; KLEBANOFF MODES; INSTABILITY; FLOW; DISTORTION;
EVOLUTION
AB This paper is concerned with the transition to turbulence in flat plate boundary layers due to moderately high levels of free-stream turbulence. The turbulence is assumed to be generated by an (idealized) grid and matched asymptotic expansions are used to analyse the resulting flow over a finite thickness flat plate located in the downstream region. The characteristic Reynolds number R-Lambda based on the mesh size. and free-stream velocity is assumed to be large, and the turbulence intensity e is assumed to be small. The asymptotic flow structure is discussed for the generic case where the turbulence Reynolds number epsilon R-Lambda and the plate thickness and are held fixed (at O(1) and O(Lambda), respectively) in the limit as R-Lambda -> infinity and epsilon -> 0. But various limiting cases are considered in order to explain the relevant transition mechanisms. It is argued that there are two types of streak-like structures that can play a role in the transition process: (i) those that appear in the downstream region and are generated by streamwise vorticity in upstream flow and (ii) those that are concentrated near the leading edge and are generated by plate normal vorticity in upstream flow. The former are relatively unaffected by leading edge geometry and are usually referred to as Klebanoff modes while the latter are strongly affected by leading edge geometry and are more streamwise vortex-like in appearance.
C1 NASA Glenn Res Ctr, Cleveland, OH 44135 USA.
RP Goldstein, ME (reprint author), NASA Glenn Res Ctr, 2100 Brookpk Rd, Cleveland, OH 44135 USA.
EM marvin.e.goldstein@nasa.gov
FU NASA Aerosciences Project
FX This work was supported by the NASA Aerosciences Project.
NR 35
TC 4
Z9 4
U1 3
U2 8
PU ROYAL SOC
PI LONDON
PA 6-9 CARLTON HOUSE TERRACE, LONDON SW1Y 5AG, ENGLAND
SN 1364-503X
EI 1471-2962
J9 PHILOS T R SOC A
JI Philos. Trans. R. Soc. A-Math. Phys. Eng. Sci.
PD JUL 28
PY 2014
VL 372
IS 2020
SI SI
AR 20130354
DI 10.1098/rsta.2013.0354
PG 18
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA AK5AW
UT WOS:000338437200012
ER
PT J
AU Rind, D
Jonas, J
Balachandran, NK
Schmidt, GA
Lean, J
AF Rind, D.
Jonas, J.
Balachandran, N. K.
Schmidt, G. A.
Lean, J.
TI The QBO in two GISS global climate models: 1. Generation of the QBO
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
ID QUASI-BIENNIAL OSCILLATION; GRAVITY-WAVE PARAMETERIZATION; DOUBLED CO2
CLIMATE; EARTH SYSTEM MODEL; MIDDLE ATMOSPHERE; CIRCULATION MODEL;
TROPICAL PRECIPITATION; CUMULUS CONVECTION; SIMULATED CLIMATE;
EQUATORIAL WAVES
AB The adjustment of parameterized gravity waves associated with model convection and finer vertical resolution has made possible the generation of the quasi-biennial oscillation (QBO) in two Goddard Institute for Space Studies (GISS) models, GISS Middle Atmosphere Global Climate Model III and a climate/middle atmosphere version of Model E2. Both extend from the surface to 0.002 hPa, with 2 degrees x 2.5 degrees resolution and 102 layers. Many realistic features of the QBO are simulated, including magnitude and variability of its period and amplitude. The period itself is affected by the magnitude of parameterized convective gravity wave momentum fluxes and interactive ozone (which also affects the QBO amplitude and variability), among other forcings. Although varying sea surface temperatures affect the parameterized momentum fluxes, neither aspect is responsible for the modeled variation in QBO period. Both the parameterized and resolved waves act to produce the respective easterly and westerly wind descent, although their effect is offset in altitude at each level. The modeled and observed QBO influences on tracers in the stratosphere, such as ozone, methane, and water vapor are also discussed. Due to the link between the gravity wave parameterization and the models' convection, and the dependence on the ozone field, the models may also be used to investigate how the QBO may vary with climate change.
C1 [Rind, D.; Schmidt, G. A.] NASA, Goddard Space Flight Ctr, Inst Space Studies, New York, NY 10025 USA.
[Jonas, J.; Balachandran, N. K.] Columbia Univ, Ctr Climate Change Res, New York, NY USA.
[Lean, J.] US Naval Res Lab, Washington, DC USA.
RP Rind, D (reprint author), NASA, Goddard Space Flight Ctr, Inst Space Studies, New York, NY 10025 USA.
EM david.h.rind@nasa.gov
RI Schmidt, Gavin/D-4427-2012
OI Schmidt, Gavin/0000-0002-2258-0486
FU NASA Glory Mission; NASA Modeling, Analysis and Prediction program
FX This paper was improved substantially by the knowledgeable suggestions
of three anonymous reviewers. We thank them greatly for all their
efforts. The work was funded by the NASA Glory Mission. Climate modeling
at GISS is supported by the NASA Modeling, Analysis and Prediction
program and resources supporting this work were provided by the NASA
High-End Computing (HEC) Program through the NASA Center for Climate
Simulation (NCCS) at Goddard Space Flight Center and the NASA program at
Ames Research Center. Data from these runs are available from Jeff Jonas
(jeffjonas88@gmail.com).
NR 81
TC 6
Z9 6
U1 0
U2 7
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 JUL 27
PY 2014
VL 119
IS 14
BP 8798
EP 8824
DI 10.1002/2014JD021678
PG 27
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA AN2GQ
UT WOS:000340402800017
ER
PT J
AU Hansell, RA
Tsay, SC
Pantina, P
Lewis, JR
Ji, Q
Herman, JR
AF Hansell, R. A.
Tsay, S. -C.
Pantina, P.
Lewis, J. R.
Ji, Q.
Herman, J. R.
TI Spectral derivative analysis of solar spectroradiometric measurements:
Theoretical basis
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
ID INFRARED RADIOMETRIC MEASUREMENTS; TRANSMITTANCE MEASUREMENTS;
MICROPHYSICAL PROPERTIES; RADIATIVE IMPACTS; RETRIEVAL METHOD; TROPICAL
CIRRUS; SOUTHEAST-ASIA; OPTICAL DEPTH; CLOUDS; AEROSOLS
AB Spectral derivative analysis, a commonly used tool in analytical spectroscopy, is described for studying cirrus clouds and aerosols using hyperspectral, remote sensing data. The methodology employs spectral measurements from the 2006 Biomass-burning Aerosols in Southeast Asia field study to demonstrate the approach. Spectral peaks associated with the first two derivatives of measured/modeled transmitted spectral fluxes are examined in terms of their shapes, magnitudes, and positions from 350 to 750nm, where variability is largest. Differences in spectral features between media are mainly associated with particle size and imaginary term of the complex refractive index. Differences in derivative spectra permit cirrus to be conservatively detected at optical depths near the optical thin limit of similar to 0.03 and yield valuable insight into the composition and hygroscopic nature of aerosols. Biomass-burning smoke aerosols/cirrus generally exhibit positive/negative slopes, respectively, across the 500-700 nm spectral band. The effect of cirrus in combined media is to increase/decrease the slope as cloud optical thickness decreases/increases. For thick cirrus, the slope tends to 0. An algorithm is also presented which employs a two model fit of derivative spectra for determining relative contributions of aerosols/clouds to measured data, thus enabling the optical thickness of the media to be partitioned. For the cases examined, aerosols/clouds explain similar to 83%/17% of the spectral signatures, respectively, yielding a mean cirrus cloud optical thickness of 0.08 +/- 0.03, which compared reasonably well with those retrieved from a collocated Micropulse Lidar Network Instrument (0.09 +/- 0.04). This method permits extracting the maximum informational content from hyperspectral data for atmospheric remote sensing applications.
C1 [Hansell, R. A.] Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20742 USA.
[Hansell, R. A.; Tsay, S. -C.; Pantina, P.; Lewis, J. R.; Ji, Q.; Herman, J. R.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Pantina, P.] Sci Syst & Applicat Inc, Lanham, MD USA.
[Lewis, J. R.; Herman, J. R.] Univ Maryland Baltimore Cty, Joint Ctr Earth Syst Technol, Baltimore, MD 21228 USA.
[Ji, Q.] Sigma Space Corp, Greenbelt, MD USA.
RP Hansell, RA (reprint author), Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20742 USA.
EM Richard.A.Hansell@nasa.gov
OI Herman, Jay/0000-0002-9146-1632
FU NASA Radiation Sciences Program; NASA Earth Observing System and
Radiation Sciences Program
FX This work is supported by the NASA Radiation Sciences Program managed by
Hal B. Maring. Both AERONET and MPLNET are funded by the NASA Earth
Observing System and Radiation Sciences Program. We would like to thank
B. Holben for establishing and maintaining the AERONET site at Phimai
and for the valuable discussions. We acknowledge the MODTRAN developers
(a joint collaboration of Spectral Sciences, Inc. and the U. S. Air
Force) for their RTM code and M. Hess for making the OPAC database
publicly available. We would like to thank G. Fager at PANalytical NIR
(formerly ASD) for his technical support of our FieldSpec Pro instrument
and D. Feldman and T. O'Haven for their MODTRANwrapper and
signal-processing codes (terpconnect.umd.edu/similar to
toh/spectrum/SignalProcessingTools.html), respectively. We also thank B.
Baum, P. Yang, A. Heymsfield, and C. Schmitt for their ice cloud
scattering models. Lastly, we thank the reviewers for their helpful and
insightful comments.
NR 57
TC 1
Z9 1
U1 1
U2 5
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 JUL 27
PY 2014
VL 119
IS 14
BP 8908
EP 8924
DI 10.1002/2013JD021423
PG 17
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA AN2GQ
UT WOS:000340402800023
ER
PT J
AU Wood, NB
L'Ecuyer, TS
Heymsfield, AJ
Stephens, GL
Hudak, DR
Rodriguez, P
AF Wood, Norman B.
L'Ecuyer, Tristan S.
Heymsfield, Andrew J.
Stephens, Graeme L.
Hudak, David R.
Rodriguez, Peter
TI Estimating snow microphysical properties using collocated multisensor
observations
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
ID PARTICLE TERMINAL VELOCITIES; ICE-CLOUD PARTICLES; VIDEO DISDROMETER;
FALL SPEEDS; PRECIPITATION; CRYSTALS; MICROWAVE; UNCERTAINTIES; CIRRUS;
AREA
AB The ability of ground-based in situ and remote sensing observations to constrain microphysical properties for dry snow is examined using a Bayesian optimal estimation retrieval method. Power functions describing the variation of mass and horizontally projected area with particle size and a parameter related to particle shape are retrieved from near-Rayleigh radar reflectivity, particle size distribution, snowfall rate, and size-resolved particle fall speeds. Algorithm performance is explored in the context of instruments deployed during the Canadian CloudSat CALIPSO Validation Project, but the algorithm is adaptable to other similar combinations of sensors. Critical estimates of observational and forward model uncertainties are developed and used to quantify the performance of the method using synthetic cases developed from actual observations of snow events. In addition to illustrating the technique, the results demonstrate that this combination of sensors provides useful constraints on the mass parameters and on the coefficient of the area power function but only weakly constrains the exponent of the area power function and the shape parameter. Information content metrics show that about two independent quantities are measured by the suite of observations and that the method is able to resolve about eight distinct realizations of the state vector containing the mass and area power function parameters. Alternate assumptions about observational and forward model uncertainties reveal that improved modeling of particle fall speeds could contribute substantial improvements to the performance of the method.
C1 [Wood, Norman B.] Univ Wisconsin, Cooperat Inst Meteorol Satellite Studies, Madison, WI 53706 USA.
[L'Ecuyer, Tristan S.] Univ Wisconsin, Dept Atmospher & Ocean Sci, Madison, WI USA.
[Heymsfield, Andrew J.] Natl Ctr Atmospher Res, Boulder, CO 80307 USA.
[Stephens, Graeme L.] NASA, Jet Prop Lab, Pasadena, CA USA.
[Hudak, David R.; Rodriguez, Peter] Environm Canada, Cloud Phys & Severe Weather Res Sect, King City, ON, Canada.
RP Wood, NB (reprint author), Univ Wisconsin, Cooperat Inst Meteorol Satellite Studies, Madison, WI 53706 USA.
EM norman.wood@ssec.wisc.edu
RI L'Ecuyer, Tristan/E-5607-2012
OI L'Ecuyer, Tristan/0000-0002-7584-4836
FU National Aeronautics and Space Administration; JPL CloudSat Office; NASA
Global Precipitation Measurement program [NN-X13AH73G]
FX Parts of this research by N.B.W. and T. S. L. were performed at the
University of Wisconsin-Madison and at Colorado State University for the
Jet Propulsion Laboratory, California Institute of Technology, sponsored
by the National Aeronautics and Space Administration. A.J.H.
acknowledges support from the JPL CloudSat Office and NASA Global
Precipitation Measurement program contract NN-X13AH73G. Thanks to G.-J.
Huang of Colorado State University (2DVD data), F. Fabry of McGill
University (VertiX data), and L. Bliven of NASA Goddard Space Flight
Center (SVI data) for making their C3VP data sets available and sharing
their expertise. Other data used in the analyses, including the relevant
FD12P and DFIR observations, are available from the authors. Thanks to
two anonymous reviewers and S. Nesbitt of University of Illinois
Urbana-Champaign for their thoughtful comments and suggestions.
NR 48
TC 12
Z9 12
U1 0
U2 16
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 JUL 27
PY 2014
VL 119
IS 14
BP 8941
EP 8961
DI 10.1002/2013JD021303
PG 21
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA AN2GQ
UT WOS:000340402800025
ER
PT J
AU Lebsock, M
Su, H
AF Lebsock, Matthew
Su, Hui
TI Application of active spaceborne remote sensing for understanding biases
between passive cloud water path retrievals
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
ID COMMUNITY ATMOSPHERE MODEL; DROPLET EFFECTIVE RADIUS; OPTICAL DEPTH;
A-TRAIN; PART II; ALGORITHM; OCEAN; PRECIPITATION; RADAR; SURFACE
AB Bias between the Advanced Microwave Scanning Radiometer-EOS (AMSR-E) version 2 and the Moderate Resolution Imaging Spectroradiometer (MODIS) collection 5.1 cloud liquid water path (W-c) products are explored with the aid of coincident active observations from the CloudSat radar and the CALIPSO lidar. In terms of detection, the active observations provide precise separation of cloudy from clear sky and precipitating from nonprecipitating clouds. In addition, they offer a unique quantification of precipitation water path (W-p) in warm clouds. They also provide an independent quantification of W-c that is based on an accurate surface reference technique, which is an independent arbiter between the two passive approaches. The results herein establish the potential for CloudSat and CALIPSO to provide an independent assessment of bias between the conventional passive remote sensing methods from reflected solar and emitted microwave radiation. After applying a common data filter to the observations to account for sampling biases, AMSR-E is biased high relative to MODIS in the global mean by 26.4 gm(-2). The RMS difference in the regional patterns is 32.4 gm(-2), which highlights a large geographical dependence in the bias which is related to the tropical transitions from stratocumulus to cumulus cloud regimes. The contributions of four potential sources for this bias are investigated by exploiting the active observations: (1) bias in MODIS related to solar zenith angle dependence accounts for -2.3 gm(-2), (2) bias in MODIS due to undersampling of cloud edges accounts for 4.2 gm(-2), (3) a wind speed and water vapor-dependent "clear-sky biase" in the AMSR-E retrieval accounts for 6.3 gm(-2), and (4) evidence suggests that much of the remaining 18 gm(-2) bias is related to the assumed partitioning of the observed emission signal between cloud and precipitation water in the AMSR-E retrieval. This is most evident through the correlations between the regional mean patterns of W-p and the W-c bias within the latitudes of 30 degrees N and 30 degrees S, suggesting that the assumption of a regionally invariant cloud/precipitation partitioning in the AMSR-E algorithm is the likely causal factor.
C1 [Lebsock, Matthew; Su, Hui] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
RP Lebsock, M (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
EM matthew.d.lebsock@jpl.nasa.gov
FU NASA
FX 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. Funding
was provided by the NASA Making Earth System Data Records for Use in
Research Environments. CloudSat data were acquired through the CloudSat
Data Processing Center at Colorado State University and can be accessed
through their Web site http://www.cloudsat.cira.colostate.edu. MODIS
products were obtained from the Goddard Distributed Active Archive
Center. AMSR-E data were acquired from the National Snow and Ice Data
Center. We are especially grateful to the three anonymous reviewers who
helped clarify the limitations of the non-overlapping AMSR-E and
CloudSat footprints and the importance of the cloud/precipitation
partitioning in the AMSR-E results.
NR 47
TC 11
Z9 11
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 JUL 27
PY 2014
VL 119
IS 14
BP 8962
EP 8979
DI 10.1002/2014JD021568
PG 18
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA AN2GQ
UT WOS:000340402800026
ER
PT J
AU Jethva, H
Torres, O
Ahn, C
AF Jethva, Hiren
Torres, Omar
Ahn, Changwoo
TI Global assessment of OMI aerosol single-scattering albedo using
ground-based AERONET inversion
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
ID OPTICAL-PROPERTIES; NON-SPHERICITY; DUST; ABSORPTION; SATELLITE;
INSTRUMENT; AIRCRAFT; NETWORK; DEPTH; SUN
AB We compare the aerosol single-scattering albedo (SSA) retrieved by the near-UV two-channel algorithm (OMAERUV) applied to the Aura/Ozone Monitoring Instrument (OMI) measurements with an equivalent inversion made by the ground-based Aerosol Robotic Network (AERONET). A recent upgrade of the OMAERUV algorithm incorporates a modified carbonaceous aerosol model, a Cloud-Aerosol Lidar with Orthogonal Polarization-based aerosol height climatology, and a robust aerosol-type identification. This paper is the first comprehensive effort to globally compare the OMI-retrieved SSA with that of AERONET using all available sites spanning the regions of biomass burning, dust, and urban pollution. An analysis of the colocated retrievals over 269 sites reveals that about 46% (69%) of OMI-AERONET matchups agree within the absolute difference of +/- 0.03 (+/- 0.05) for all aerosol types. The comparison improves to 52% (77%) when only "smoke" and "dust" aerosol types were identified by the OMAERUV algorithm. Regionally, the agreement between the two inversions was robust over the biomass burning sites of South America, Sahel, Indian subcontinent, and oceanic/coastal sites followed by a reasonable agreement over Northeast Asia. Over the desert regions, OMI tends to retrieve higher SSA, particularly over the Arabian Peninsula. Globally, the OMI-AERONET matchups agree mostly within +/- 0.03 for the aerosol optical depth (440 nm) and UV-aerosol index larger than 0.4 and 1.0, respectively. Possible sources of uncertainty in the OMI retrieval can be the subpixel cloud contamination, assumptions of the surface albedo, and spectral aerosol absorption. We expect further refinement in the OMAERUV algorithm which stands uniquely in characterizing aerosol absorption from space.
C1 [Jethva, Hiren] Univ Space Res Assoc, Columbia, MD 21046 USA.
[Jethva, Hiren; Torres, Omar] NASA, Goddard Space Flight Ctr, Lab Atmospher Chem & Dynam, Greenbelt, MD 20771 USA.
[Ahn, Changwoo] Sci Syst & Applicat Inc, Lanham, MD USA.
RP Jethva, H (reprint author), Univ Space Res Assoc, Columbia, MD 21046 USA.
EM hiren.t.jethva@nasa.gov
RI Torres, Omar/G-4929-2013
NR 37
TC 20
Z9 20
U1 0
U2 10
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 JUL 27
PY 2014
VL 119
IS 14
BP 9020
EP 9040
DI 10.1002/2014JD021672
PG 21
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA AN2GQ
UT WOS:000340402800029
ER
PT J
AU Schmitt, MP
Rai, AK
Bhattacharya, R
Zhu, DM
Wolfe, DE
AF Schmitt, Michael P.
Rai, Amarendra K.
Bhattacharya, Rabi
Zhu, Dongming
Wolfe, Douglas E.
TI "Multilayer thermal barrier coating (TBC) architectures utilizing rare
earth doped YSZ and rare earth pyrochlores"
SO SURFACE & COATINGS TECHNOLOGY
LA English
DT Article
DE Thermal barrier coating; TBC; Pyrochlore; Multilayer; Rare earth
ID CONDUCTIVITY
AB To allow for increased gas turbine efficiencies, new insulating thermal barrier coatings (TBCs) must be developed to protect the underlying metallic components from higher operating temperatures. This work focused on using rare earth doped (Yb and Gd) yttria stabilized zirconia (t' low-k) and Gd2Zr2O7 pyrochlores (GZO) combined with novel nanolayered and thick layered microstructures to enable operation beyond the 1200 degrees C stability limit of current 7 wt.% yttria stabilized zirconia (7YSZ) coatings. It was observed that the layered system can reduce the thermal conductivity by similar to 45% with respect to YSZ after 20 h of testing at 1316 degrees C. The erosion rate of GZO is shown to be an order to magnitude higher than YSZ and t' low-k, but this can be reduced by almost 57% when utilizing a nanolayered structure. Lastly, the thermal instability of the layered system is investigated and thought is given to optimization of layer thickness. (C) 2014 Elsevier B.V. All rights reserved.
C1 [Schmitt, Michael P.; Wolfe, Douglas E.] Penn State Univ, Appl Res Lab, University Pk, PA 16802 USA.
[Schmitt, Michael P.; Wolfe, Douglas E.] Penn State Univ, Dept Mat Sci & Engn, University Pk, PA 16802 USA.
[Rai, Amarendra K.; Bhattacharya, Rabi] UES Inc, Dayton, OH 45432 USA.
[Zhu, Dongming] NASA Glenn Res Ctr, Cleveland, OH 44135 USA.
RP Wolfe, DE (reprint author), Penn State Univ, Appl Res Lab, University Pk, PA 16802 USA.
EM dew125@arl.psu.edu
FU DOE STTR Phase II [DE-SC0005356]; Eric Walker fellowship program of the
Applied Research Laboratory at the Pennsylvania State University
FX The authors would like to thank Anna Stump for help with sample
preparation and microscopy and Ethan Lucas for help with coating erosion
testing. This work was funded in part under DOE STTR Phase II award No.
DE-SC0005356 and the Eric Walker fellowship program of the Applied
Research Laboratory at the Pennsylvania State University. Any opinions,
findings, conclusions, or recommendations expressed in this material are
those of the authors and do not necessarily reflect the views of the
DOE.
NR 19
TC 13
Z9 13
U1 6
U2 50
PU ELSEVIER SCIENCE SA
PI LAUSANNE
PA PO BOX 564, 1001 LAUSANNE, SWITZERLAND
SN 0257-8972
J9 SURF COAT TECH
JI Surf. Coat. Technol.
PD JUL 25
PY 2014
VL 251
BP 56
EP 63
DI 10.1016/j.surfcoat.2014.03.049
PG 8
WC Materials Science, Coatings & Films; Physics, Applied
SC Materials Science; Physics
GA AJ8XT
UT WOS:000337992100008
ER
PT J
AU Henderson, BL
Gudipati, MS
AF Henderson, Bryana L.
Gudipati, Murthy S.
TI Plume Composition and Evolution in Multicomponent Ices Using Resonant
Two-Step Laser Ablation and Ionization Mass Spectrometry
SO JOURNAL OF PHYSICAL CHEMISTRY A
LA English
DT Article
ID MOLECULAR-DYNAMICS SIMULATIONS; KNUDSEN-LAYER FORMATION; DESORPTION
IONIZATION; ORGANIC-SOLIDS; UV-MALDI; ION YIELDS; 248 NM; MATRIX;
CLUSTERS; MECHANISMS
AB The composition and evolution of plumes generated in a resonant infrared (IR) laser desorption of low-temperature ices is investigated via a recently developed two-step laser desorption and ionization mass spectrometry (2S-LAIMS) technique where a neutral plume is ejected by an IR laser pulse and ionized by a UV laser pulse for analysis via time-of-flight mass spectrometry. By varying the delay between the lasers, we can construct a complete time-resolved model of the ejected plume components. We found that water ices containing mixtures of polar and nonpolar analytes displayed complex mass spectral profiles that varied as the plume evolved. In these samples, the low-volatility polar analytes and clusters were restricted to the early part of the plume, whereas volatile or nonpolar analytes were spread throughout the plume. The distributions of low-volatility polar species, clusters, and impurities from the copper substrate were well-represented by single Maxwell-like distributions centered at high velocities (600-800 m s(-1)), while nonpolar, volatile species contained two distinct components, indicating both ablation and thermal desorption processes. Characterization of plume distributions can therefore provide new insight into an analyte's chemical identity and can aid in assignment of otherwise ambiguous signals in the mass spectra.
C1 [Henderson, Bryana L.; Gudipati, Murthy S.] CALTECH, Jet Prop Lab, Div Sci, Pasadena, CA 91109 USA.
RP Gudipati, MS (reprint author), CALTECH, Jet Prop Lab, Div Sci, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM gudipati@jpl.nasa.gov
RI Gudipati, Murthy/F-7575-2011
FU JPL's DRDF; JPL's RTD; NASA Spitzer Science Center; NASA; Europa Clipper
Pre-Project; National Aeronautics and Space Administration; NASA
Postdoctoral Program for an NPP fellowship
FX This research was enabled through partial funding from JPL's DRDF and
R&TD funding for infrastructure of the "Ice Spectroscopy Laboratory" at
JPL, NASA Spitzer Science Center, NASA funding through Planetary
Atmospheres, and the Europa Clipper Pre-Project. This research was
carried out at the Jet Propulsion Laboratory, California Institute of
Technology, under a contract with the National Aeronautics and Space
Administration. B.L.H. acknowledges funding from the NASA Postdoctoral
Program for an NPP fellowship. We thank Dr. Robert Wagner (Karlsruhe
Institute of Technology, Germany) for assisting with the LabVIEW
software integration of the experimental setup. B.L.H. is a NASA
Postdoctoral Fellow at the Jet Propulsion Laboratory. M.S.G. is also a
Senior Research Scientist at the IPST, University of Maryland at College
Park.
NR 47
TC 2
Z9 2
U1 1
U2 8
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 JUL 24
PY 2014
VL 118
IS 29
BP 5454
EP 5463
DI 10.1021/jp503111k
PG 10
WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical
SC Chemistry; Physics
GA AM0MU
UT WOS:000339540500011
PM 24990519
ER
PT J
AU Liao, YL
Chen, ZF
Connell, JW
Fay, CC
Park, C
Kim, JW
Lin, Y
AF Liao, Yunlong
Chen, Zhongfang
Connell, John W.
Fay, Catharine C.
Park, Cheol
Kim, Jae-Woo
Lin, Yi
TI Chemical Sharpening, Shortening, and Unzipping of Boron Nitride
Nanotubes
SO ADVANCED FUNCTIONAL MATERIALS
LA English
DT Article
ID WALLED CARBON NANOTUBES; GRAPHENE NANORIBBONS; POLYMERIC COMPOSITES;
FACILE SYNTHESIS; BN NANOTUBES; NANOSHEETS; FUNCTIONALIZATION;
PURIFICATION; SOLUBILIZATION; OXIDATION
AB Boron nitride nanotubes (BNNTs), the one-dimensional member of the boron nitride nanostructure family, are generally accepted to be highly inert to oxidative treatments and can only be covalently modified by highly reactive species. Conversely, it is discovered that the BNNTs can be chemically dispersed and their morphology modified by a relatively mild method: simply sonicating the nanotubes in aqueous ammonia solution. The dispersed nanotubes are significantly corroded, with end-caps removed, tips sharpened, and walls thinned. The sonication treatment in aqueous ammonia solution also removes amorphous BN impurities and shortened BNNTs, resembling various oxidative treatments of carbon nanotubes. Importantly, the majority of BNNTs are at least partially longitudinally cut, or "unzipped". Entangled and freestanding BN nanoribbons (BNNRs), resulting from the unzipping, are found to be similar to 5-20 nm in width and up to a few hundred nanometers in length. This is the first chemical method to obtain BNNRs from BNNT unzipping. This method is not derived from known carbon nanotube unzipping strategies, but is unique to BNNTs because the use of aqueous ammonia solutions specifically targets the B-N bond network. This study may pave the way for convenient processing of BNNTs, previously thought to be highly inert, toward controlling their dispersion, purity, lengths, and electronic properties.
C1 [Liao, Yunlong; Kim, Jae-Woo; Lin, Yi] Natl Inst Aerosp, Hampton, VA 23666 USA.
[Liao, Yunlong; Chen, Zhongfang] Univ Puerto Rico, Dept Phys, Dept Chem, San Juan, PR 00931 USA.
[Connell, John W.; Fay, Catharine C.; Park, Cheol] NASA, Langley Res Ctr, Hampton, VA 23681 USA.
[Park, Cheol] Univ Virginia, Dept Mech & Aerosp Engn, Charlottesville, VA 22904 USA.
[Lin, Yi] Coll William & Mary, Dept Appl Sci, Williamsburg, VA 23185 USA.
RP Liao, YL (reprint author), Natl Inst Aerosp, 100 Explorat Way, Hampton, VA 23666 USA.
EM zhongfangchen@gmail.com; john.w.connell@nasa.gov; yi.lin@nianet.org
RI Kim, Jae-Woo/A-8314-2008; Chen, Zhongfang/A-3397-2008
FU Department of Defense [W911NF-12-1-0083]; NASA [NNX10AM80H, NNX13AB22A];
US Air Force Office of Scientific Research - Low Density Materials
program [FA9550-11-1-0042]
FX We thank Dr. W. Cao and Prof. H. Elsayed-Ali (Applied Research Center,
Old Dominion University) for assistance in HR-TEM imaging and C.
Chamberlain (NASA Langley Research Center) for TGA measurements. Y. Liao
was an exchange student resident from University of Puerto Rico, who is
supported by Department of Defense (Grant W911NF-12-1-0083) and NASA
(Grant Nos. NNX10AM80H and NNX13AB22A) to conduct research at National
Institute of Aerospace and NASA Langley Research Center. C. Park
acknowledges the financial support in part by US Air Force Office of
Scientific Research - Low Density Materials program (Grant No.
FA9550-11-1-0042).
NR 56
TC 12
Z9 12
U1 2
U2 81
PU WILEY-V C H VERLAG GMBH
PI WEINHEIM
PA BOSCHSTRASSE 12, D-69469 WEINHEIM, GERMANY
SN 1616-301X
EI 1616-3028
J9 ADV FUNCT MATER
JI Adv. Funct. Mater.
PD JUL 23
PY 2014
VL 24
IS 28
BP 4497
EP 4506
DI 10.1002/adfm.201400599
PG 10
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 AM2XE
UT WOS:000339713900014
ER
PT J
AU Williams, JC
Meador, MAB
McCorkle, L
Mueller, C
Wilmoth, N
AF Williams, Jarrod C.
Meador, Mary Ann B.
McCorkle, Linda
Mueller, Carl
Wilmoth, Nathan
TI Synthesis and Properties of Step-Growth Polyamide Aerogels Cross-linked
with Triacid Chlorides
SO CHEMISTRY OF MATERIALS
LA English
DT Article
ID SYNDIOTACTIC POLYSTYRENE AEROGELS; POLYIMIDE AEROGELS;
POLYACRYLAMIDE-GELS; MECHANICALLY STRONG; SILICA AEROGELS; CARBON
AEROGELS; ADSORPTION; STRENGTH
AB We report the first synthesis of step-growth aromatic polyamide (PA) aerogels made using amine end-capped polyamide oligomers cross-linked with 1,3,5-benzenetricarbonyl trichloride (BTC). Isophthaloyl chloride (IPC) or terephthaloyl chloride (TPC) were combined with m-phenylenediamine (mPDA) in N-methylpyrrolidinone (NMP) to give amine-capped polyamide oligomers formulated with up to 40 repeat units. Addition of the cross-linker, BTC, typically induces gelation in under 5 min. Solvent exchange of the resulting gels into ethanol followed by supercritical CO2 drying gives colorless aerogels with densities ranging from 0.06 to 0.33 g/cm(3), compressive moduli between 5 and 312 MPa, and surface areas as high as 385 m(2)/g. Dielectric properties were also measured in the X-band frequency range. It was found that relative dielectric constant decreased with density as seen with other aerogels with the lowest relative dielectric constant being 1.15 for aerogels with densities of 0.06 g/cm(3). Because of their superior mechanical properties, these aerogels can be utilized in a number of aerospace related applications, such as insulation for rovers, habitats, deployable structures, and extravehicular activity suits, as well as low dielectric substrates for antennas and other electronics. Because of potentially lower cost relative to polyimide and other polymer aerogels, they also have potential for use in more terrestrial applications as well, such as insulation for refrigeration, building and construction, and protective clothing.
C1 [Williams, Jarrod C.] NASA Glenn Res Ctr, NASA Postdoctoral Program, Cleveland, OH 44135 USA.
[Meador, Mary Ann B.] NASA Glenn Res Ctr, Mat & Struct Div, Cleveland, OH 44135 USA.
[McCorkle, Linda] Ohio Aerosp Inst, Cleveland, OH 44142 USA.
[Mueller, Carl] Qinetiq NA, Waltham, MA 02451 USA.
[Wilmoth, Nathan] Vantage Partners LLC, Brookpark, OH 44142 USA.
RP Williams, JC (reprint author), NASA Glenn Res Ctr, NASA Postdoctoral Program, 21000 Brookpk Rd, Cleveland, OH 44135 USA.
EM jarrod.c.williams@nasa.gov; maryann.meador@nasa.gov
OI Meador, Mary Ann/0000-0003-2513-7372
NR 34
TC 21
Z9 22
U1 7
U2 75
PU AMER CHEMICAL SOC
PI WASHINGTON
PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA
SN 0897-4756
EI 1520-5002
J9 CHEM MATER
JI Chem. Mat.
PD JUL 22
PY 2014
VL 26
IS 14
BP 4163
EP 4171
DI 10.1021/cm5012313
PG 9
WC Chemistry, Physical; Materials Science, Multidisciplinary
SC Chemistry; Materials Science
GA AL9OU
UT WOS:000339471400018
ER
PT J
AU Gastaldello, F
Limousin, M
Foex, G
Munoz, RP
Verdugo, T
Motta, V
More, A
Cabanac, R
Buote, DA
Eckert, D
Ettori, S
Fritz, A
Ghizzardi, S
Humphrey, PJ
Meneghetti, M
Rossetti, M
AF Gastaldello, F.
Limousin, M.
Foex, G.
Munoz, R. P.
Verdugo, T.
Motta, V.
More, A.
Cabanac, R.
Buote, D. A.
Eckert, D.
Ettori, S.
Fritz, A.
Ghizzardi, S.
Humphrey, P. J.
Meneghetti, M.
Rossetti, M.
TI Dark matter-baryons separation at the lowest mass scale: the Bullet
Group
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE gravitational lensing: strong; galaxies: groups: individual: SL2S
J08544-0121; dark matter; X-rays: galaxies: clusters
ID GALAXY CLUSTER MERGER; SAMPLE; DYNAMICS; RELEASE
AB We report on the X-ray observation of a strong lensing selected group, SL2S J08544-0121, with a total mass of 2.4 +/- 0.6 x 10(14) M-circle dot which revealed a separation of 124 +/- 20 kpc between the X-ray emitting collisional gas and the collisionless galaxies and dark matter (DM), traced by strong lensing. This source allows to put an order of magnitude estimate to the upper limit to the interaction cross-section of DM of 10 cm(2) g(-1). It is the lowest mass object found to date showing a DM-baryons separation, and it reveals that the detection of bullet-like objects is not rare and confined to mergers of massive objects opening the possibility of a statistical detection of DM-baryons separation with future surveys.
C1 [Gastaldello, F.; Eckert, D.; Fritz, A.; Ghizzardi, S.; Rossetti, M.] INAF IASF Milano, I-20133 Milan, Italy.
[Gastaldello, F.; Buote, D. A.; Humphrey, P. J.] Univ Calif Irvine, Dept Phys & Astron, Irvine, CA 92697 USA.
[Limousin, M.] Aix Marseille Univ, CNRS, LAM, UMR 7326, F-13388 Marseille, France.
[Limousin, M.] Univ Copenhagen, Niels Bohr Inst, Dark Cosmol Ctr, DK-2100 Copenhagen, Denmark.
[Foex, G.; Motta, V.] Univ Valparaiso, Inst Fis & Astron, Valparaiso 2360102, Chile.
[Munoz, R. P.] Pontificia Univ Catolica Chile, Fac Fis, Inst Astrofis, Santiago 7820436, Chile.
[Verdugo, T.] Ctr Invest Astron, Merida 5101A, Venezuela.
[More, A.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA.
[More, A.] Univ Tokyo, Kavli IPMU, Kashiwa, Chiba 2778583, Japan.
[Cabanac, R.] Univ Toulouse UPS, CNRS, Inst Rech Astrophys & Planetol, F-65000 Tarbes, France.
[Eckert, D.] Univ Geneva, Astron Observ, CH-1290 Versoix, Switzerland.
[Ettori, S.; Meneghetti, M.] INAF, Osservatorio Astron Bologna, I-40127 Bologna, Italy.
[Ettori, S.; Meneghetti, M.] Ist Nazl Fis Nucl, Sez Bologna, I-40127 Bologna, Italy.
[Meneghetti, M.] JPL, Pasadena, CA 91109 USA.
[Rossetti, M.] Univ Milan, Dip Fis, I-20133 Milan, Italy.
RP Gastaldello, F (reprint author), INAF IASF Milano, Via E Bassini 15, I-20133 Milan, Italy.
EM gasta@lambrate.inaf.it
RI Gastaldello, Fabio/N-4226-2015; Ettori, Stefano/N-5004-2015; Meneghetti,
Massimo/O-8139-2015;
OI Gastaldello, Fabio/0000-0002-9112-0184; Ettori,
Stefano/0000-0003-4117-8617; Meneghetti, Massimo/0000-0003-1225-7084;
Ghizzardi, Simona/0000-0003-0879-7328; Verdugo,
Tomas/0000-0003-4062-6123
FU INAF-ASI [I/023/05/0, I/088/06/0, I/032/10/0]; INAF through VIPERS;
FONDECYT [1120741, 3130750]; ECOS-CONICYT [C12U02]; CONACYT [165365,
203489]; INFN project [PD51]; [ASI/INAF/I/023/12/0]
FX FG is supported by INAF-ASI through grant I/023/05/0, I/088/06/0 and
I/032/10/0. AF is supported by INAF through VIPERS grants PRIN
2008/2010. VM acknowledges the support of FONDECYT 1120741. RM
acknowledges the support of FONDECYT 3130750. RC, GF, ML, VM acknowledge
the support of ECOS-CONICYT C12U02. TV acknowledges support from CONACYT
through grant 165365 and 203489. MM acknowledges financial contribution
from the agreement ASI/INAF/I/023/12/0 and from INFN project PD51.
NR 30
TC 10
Z9 10
U1 0
U2 5
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 JUL 21
PY 2014
VL 442
IS 1
BP L76
EP L80
DI 10.1093/mnrasl/slu058
PG 5
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AZ2DP
UT WOS:000348045200017
ER
PT J
AU Ramsay, G
Hakala, P
Howell, SB
AF Ramsay, Gavin
Hakala, Pasi
Howell, Steve B.
TI Red giant pulsations from the suspected symbiotic star StHA 169 detected
in Kepler data
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE binaries: symbiotic; Stars: individual: StHa 169; ultraviolet: stars
ID PERIOD-LUMINOSITY RELATIONS; LARGE-MAGELLANIC-CLOUD; CH-CYGNI;
WHITE-DWARF; PHOTOMETRIC CALIBRATION; RS OPHIUCHI; SPACED DATA;
VARIABILITY; CATALOG; FIELD
AB We present Kepler and Swift observations of StHa 169 which is currently classified as a symbiotic binary. The Kepler light curve shows quasi-periodic behaviour with a mean period of 34 d and an amplitude of a few per cent. Using Swift data, we find a relatively strong UV source at the position of StHa 169 but no X-ray counterpart. Using a simple two-component blackbody fit to model the combined Swift and 2MASS spectral energy distribution and an assessment of the previously published optical spectrum, we find that the source has a hot (similar to 10 000 K) component and a cooler (similar to 3700 K) component. The Kepler light is dominated by the cool component and we attribute the variability to pulsations in a red giant star. If we remove this approximate month long modulation from the light curve, we find no evidence for additional variability in the light curve. The hotter source is assigned to a late B or early A main-sequence star. We briefly discuss the implications of these findings and conclude that StHA 169 is a red giant plus main-sequence binary.
C1 [Ramsay, Gavin] Armagh Observ, Armagh BT61 9DG, North Ireland.
[Hakala, Pasi] Univ Turku, Finnish Ctr Astron ESO FINCA, FI-21500 Piikkio, Finland.
[Howell, Steve B.] NASA, Ames Res Ctr, Moffett Field, CA 94095 USA.
RP Ramsay, G (reprint author), Armagh Observ, Coll Hill, Armagh BT61 9DG, North Ireland.
EM gar@arm.ac.uk
FU NASA, Science Mission Directorate; NASA [NAS5 26555]; NASA Office of
Space Science [NAG5 7584]; Northern Ireland Government through the
Department of Culture, Arts and Leisure
FX Kepler was selected as the 10th mission of the Discovery Program.
Funding for this mission is provided by NASA, Science Mission
Directorate. The Kepler 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 NAG5 7584 and by other grants and contracts. This work made
use of PYKE, a software package for the reduction and analysis of Kepler
data. This open source software project is developed and distributed by
the NASA Kepler Guest Observer Office. Armagh Observatory is supported
by the Northern Ireland Government through the Department of Culture,
Arts and Leisure. We thank the anonymous referee for a useful report.
NR 36
TC 0
Z9 0
U1 0
U2 0
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 JUL 21
PY 2014
VL 442
IS 1
BP 489
EP 494
DI 10.1093/mnras/stu800
PG 6
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AK9RW
UT WOS:000338765400044
ER
PT J
AU Dutta, P
Chengalur, JN
Roy, N
Goss, WM
Arjunwadkar, M
Minter, AH
Brogan, CL
Lazio, TJW
AF Dutta, Prasun
Chengalur, Jayaram N.
Roy, Nirupam
Goss, W. M.
Arjunwadkar, Mihir
Minter, Anthony H.
Brogan, Crystal L.
Lazio, T. J. W.
TI The structure function of Galactic H I opacity fluctuations on au scales
based on MERLIN, VLA and VLBA data
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE turbulence; ISM: atoms; ISM: general; ISM: structure; radio lines: ISM
ID DIFFUSE INTERSTELLAR-MEDIUM; POWER SPECTRUM ANALYSIS; COLD NEUTRAL
MEDIUM; ATOMIC-STRUCTURE; MAGNETIC-FIELDS; TURBULENCE; HYDROGEN;
ABSORPTION; EMISSION; GAS
AB We use MERLIN, VLA and VLBA observations of Galactic H I absorption towards 3C 138 to estimate the structure function of the H I opacity fluctuations at au scales. Using Monte Carlo simulations, we show that there is likely to be a significant bias in the estimated structure function at signal-to-noise ratios characteristic of our observations, if the structure function is constructed in the manner most commonly used in the literature. We develop a new estimator that is free from this bias and use it to estimate the true underlying structure function slope on length-scales ranging from 5 to 40 au. From a power-law fit to the structure function, we derive a slope of 0.81(-0.13)(+0.14), i.e. similar to the value observed at parsec scales. The estimated upper limit for the amplitude of the structure function is also consistent with the measurements carried out at parsec scales. Our measurements are hence consistent with the H I opacity fluctuation in the Galaxy being characterized by a power-law structure function over length-scales that span six orders of magnitude. This result implies that the dissipation scale has to be smaller than a few au if the fluctuations are produced by turbulence. This inferred smaller dissipation scale implies that the dissipation occurs either in (i) regions with densities greater than or similar to 10(3) cm(-3) (i. e. similar to that inferred for 'tiny scale' atomic clouds or (ii) regions with a mix of ionized and atomic gas (i. e. the observed structure in the atomic gas has a magnetohydrodynamic origin).
C1 [Dutta, Prasun; Chengalur, Jayaram N.; Arjunwadkar, Mihir] Natl Ctr Radio Astrophys, Pune 411007, Maharashtra, India.
[Roy, Nirupam] Max Planck Inst Radioastron, D-53121 Bonn, Germany.
[Goss, W. M.] Natl Radio Astron Observ, Socorro, NM 87801 USA.
[Minter, Anthony H.] Natl Radio Astron Observ, Green Bank, WV 24944 USA.
[Brogan, Crystal L.] Natl Radio Astron Observ, Charlottesville, VA 22903 USA.
[Lazio, T. J. W.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Dutta, P (reprint author), Natl Ctr Radio Astrophys, Post Bag 3, Pune 411007, Maharashtra, India.
EM prasun@ncra.tifr.res.in
OI Arjunwadkar, Mihir/0000-0002-7653-8494
FU DST - INSPIRE fellowship [IFA-13 PH-54]; Alexander von Humboldt
Foundation; Jansky Fellowship of the National Radio Astronomy
Observatory; National Aeronautics and Space Administration
FX The authors are grateful to K. Subramanian, A. Deshpande, N. Kanekar, S.
Bharadwaj and S. Bhatnagar for useful discussions. This paper reports
results from observations with MERLIN, VLA and VLBA. MERLIN is a
National Facility operated by the University of Manchester at Jodrell
Bank Observatory on behalf of PPARC/STFC. The National Radio Astronomy
Observatory is a facility of the National Science Foundation operated
under cooperative agreement by Associated Universities, Inc. PD would
like to acknowledge the DST - INSPIRE fellowship [IFA-13 PH-54 dated
2013 Aug 01] used while doing this research. NR acknowledges support
from the Alexander von Humboldt Foundation and the Jansky Fellowship of
the National Radio Astronomy Observatory. 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 33
TC 3
Z9 4
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 JUL 21
PY 2014
VL 442
IS 1
BP 647
EP 655
DI 10.1093/mnras/stu881
PG 9
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AK9RW
UT WOS:000338765400055
ER
PT J
AU Thakur, N
Gopalswamy, N
Xie, H
Makela, P
Yashiro, S
Akiyama, S
Davila, JM
AF Thakur, N.
Gopalswamy, N.
Xie, H.
Maekelae, P.
Yashiro, S.
Akiyama, S.
Davila, J. M.
TI GROUND LEVEL ENHANCEMENT IN THE 2014 JANUARY 6 SOLAR ENERGETIC PARTICLE
EVENT
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; SHOCK FORMATION; RELEASE TIMES; CYCLE 24; SECCHI
AB We present a study of the 2014 January 6 solar energetic particle event which produced a small ground level enhancement (GLE), making it the second GLE of this unusual solar cycle 24. This event was primarily observed by the South Pole neutron monitors (increase of similar to 2.5%) while a few other neutron monitors recorded smaller increases. The associated coronal mass ejection (CME) originated behind the western limb and had a speed of 1960 km s(-1). The height of the CME at the start of the associated metric type II radio burst, which indicates the formation of a strong shock, was measured to be 1.61 Rs using a direct image from STEREO-A/EUVI. The CME height at the time of the GLE particle release (determined using the South Pole neutron monitor data) was directly measured as 2.96 Rs based on STEREO-A/COR1 white-light observations. These CME heights are consistent with those obtained for GLE71, the only other GLE of the current cycle, as well as cycle-23 GLEs derived using back-extrapolation. GLE72 is of special interest because it is one of only two GLEs of cycle 24, one of two behind-the-limb GLEs, and one of the two smallest GLEs of cycles 23 and 24.
C1 [Thakur, N.; Gopalswamy, N.; Xie, H.; Maekelae, P.; Yashiro, S.; Akiyama, S.; Davila, J. M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Thakur, N.; Xie, H.; Maekelae, P.; Yashiro, S.; Akiyama, S.] Catholic Univ Amer, Washington, DC 20064 USA.
RP Thakur, N (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
OI Makela, Pertti/0000-0002-8182-4559
FU European Union [213007]; National Science Foundation; NASA's LWS TRT
program
FX We thank Dr. P. Evenson of Bartol Neutron Monitor Network for the
neutron monitor asymptotic directions and useful discussions. We thank
Dr. T. Kuwabara of Bartol for his help with the conversion of the IMF
directions for Figure 3. We acknowledge the NMDB database (www.nmdb.eu),
founded under the European Union's FP7 programme (contract No. 213007)
for providing data. Neutron monitors of the Bartol Research Institute
are supported by the National Science Foundation. STEREO is a mission in
NASA's Solar Terrestrial Probes program. SOHO is a project of
international collaboration between ESA and NASA. This work was
supported by NASA's LWS TR&T program.
NR 29
TC 18
Z9 18
U1 0
U2 7
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 JUL 20
PY 2014
VL 790
IS 1
AR L13
DI 10.1088/2041-8205/790/1/L13
PG 5
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AM5ED
UT WOS:000339878100013
ER
PT J
AU An, HJ
Kaspi, VM
Beloborodov, AM
Kouveliotou, C
Archibald, RF
Boggs, SE
Christensen, FE
Craig, WW
Gotthelf, EV
Grefenstette, BW
Hailey, CJ
Harrison, FA
Madsen, KK
Mori, K
Stern, D
Zhang, WW
AF An, Hongjun
Kaspi, Victoria M.
Beloborodov, Andrei M.
Kouveliotou, Chryssa
Archibald, Robert F.
Boggs, Steven E.
Christensen, Finn E.
Craig, William W.
Gotthelf, Eric V.
Grefenstette, Brian W.
Hailey, Charles J.
Harrison, Fiona A.
Madsen, Kristin K.
Mori, Kaya
Stern, Daniel
Zhang, William W.
TI NuSTAR OBSERVATIONS OF X-RAY BURSTS FROM THE MAGNETAR 1E 1048.1-5937
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE pulsars: individual (1E 1048.1-5937); stars: magnetars; stars: neutron;
X-rays: bursts
ID SOFT GAMMA-REPEATERS; NEUTRON-STARS; SGR 1627-41; PULSAR;
1E-1048.1-5937; VARIABILITY; SGR-1900+14; QUIESCENCE; EMISSION; OUTBURST
AB We report the detection of eight bright X-ray bursts from the 6.5 s magnetar 1E 1048.1-5937, during a 2013 July observation campaign with the Nuclear Spectroscopic Telescope Array. We study the morphological and spectral properties of these bursts and their evolution with time. The bursts resulted in count rate increases by orders of magnitude, sometimes limited by the detector dead time, and showed blackbody spectra with kT 6-8 keV in the T90 duration of 1-4 s, similar to earlier bursts detected from the source. We find that the spectra during the tail of the bursts can be modeled with an absorbed blackbody with temperature decreasing with flux. The burst flux decays followed a power law of index 0.8-0.9. In the burst tail spectra, we detect a 13 keV emission feature, similar to those reported in previous bursts from this source as well as from other magnetars observed with the Rossi X-ray Timing Explorer. We explore possible origins of the spectral feature such as proton cyclotron emission, which implies a magnetic field strength of B 2x10(15) G in the emission region. However, the consistency of the energy of the feature in different objects requires further explanation.
C1 [An, Hongjun; Kaspi, Victoria M.; Archibald, Robert F.] McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada.
[Beloborodov, Andrei M.; Gotthelf, Eric V.; Hailey, Charles J.; Mori, Kaya] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA.
[Kouveliotou, Chryssa] NASA, George C Marshall Space Flight Ctr, Space Sci Off, Huntsville, AL 35812 USA.
[Boggs, Steven E.; Craig, William W.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
[Christensen, Finn E.] Tech Univ Denmark, Natl Space Inst, DTU Space, DK-2800 Lyngby, Denmark.
[Craig, William W.] Lawrence Livermore Natl Lab, Livermore, CA 94550 USA.
[Grefenstette, Brian W.; Harrison, Fiona A.; Madsen, Kristin K.] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA.
[Stern, Daniel] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Zhang, William W.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP An, HJ (reprint author), McGill Univ, Dept Phys, 3600 Univ St, Montreal, PQ H3A 2T8, Canada.
RI Boggs, Steven/E-4170-2015;
OI Boggs, Steven/0000-0001-9567-4224; An, Hongjun/0000-0002-6389-9012;
Madsen, Kristin/0000-0003-1252-4891
FU National Aeronautics and Space Administration; NSERC Discovery Grant;
FQRNT Centre de Recherche Astrophysique du Quebec; R. Howard Webster
Foundation Fellowship from the Canadian Institute for Advanced Research
(CIFAR); Canada Research Chairs Program; Lorne Trottier Chair in
Astrophysics and Cosmology; NASA [NNX10AI72G, NNX13AI34G]
FX This work was supported under NASA Contract No. NNG08FD60C, and made use
of data from the NuSTAR mission, a project led by the California
Institute of Technology, managed by the Jet Propulsion Laboratory, and
funded by the National Aeronautics and Space Administration. We thank
the NuSTAR Operations, Software and Calibration teams for support with
the execution and analysis of these observations. This research has made
use of the NuSTAR Data Analysis Software (NuSTARDAS) jointly developed
by the ASI Science Data Center (ASDC, Italy) and the California
Institute of Technology (USA). V. M. K. acknowledges support from an
NSERC Discovery Grant, the FQRNT Centre de Recherche Astrophysique du
Quebec, an R. Howard Webster Foundation Fellowship from the Canadian
Institute for Advanced Research (CIFAR), the Canada Research Chairs
Program, and the Lorne Trottier Chair in Astrophysics and Cosmology. A.
M. B. acknowledges the support by NASA grants NNX10AI72G and NNX13AI34G.
NR 37
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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 JUL 20
PY 2014
VL 790
IS 1
AR 60
DI 10.1088/0004-637X/790/1/60
PG 9
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AL0SK
UT WOS:000338836800060
ER
PT J
AU Ballard, S
Chaplin, WJ
Charbonneau, D
Desert, JM
Fressin, F
Zeng, L
Werner, MW
Davies, GR
Aguirre, VS
Basu, S
Christensen-Dalsgaard, J
Metcalfe, TS
Stello, D
Bedding, TR
Campante, TL
Handberg, R
Karoff, C
Elsworth, Y
Gilliland, RL
Hekker, S
Huber, D
Kawaler, SD
Kjeldsen, H
Lund, MN
Lundkvist, M
AF Ballard, Sarah
Chaplin, William J.
Charbonneau, David
Desert, Jean-Michel
Fressin, Francois
Zeng, Li
Werner, Michael W.
Davies, Guy R.
Aguirre, Victor Silva
Basu, Sarbani
Christensen-Dalsgaard, Jorgen
Metcalfe, Travis S.
Stello, Dennis
Bedding, Timothy R.
Campante, Tiago L.
Handberg, Rasmus
Karoff, Christoffer
Elsworth, Yvonne
Gilliland, Ronald L.
Hekker, Saskia
Huber, Daniel
Kawaler, Steven D.
Kjeldsen, Hans
Lund, Mikkel N.
Lundkvist, Mia
TI KEPLER-93b: A TERRESTRIAL WORLD MEASURED TO WITHIN 120 km, AND A TEST
CASE FOR A NEW SPITZER OBSERVING MODE
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE eclipses; methods: observational; planetary systems; stars: individual
(KOI 69, KIC 3544595)
ID TRANSIT TIMING VARIATIONS; STELLAR EVOLUTION CODE; FINE GUIDANCE SENSOR;
CIRCLE-PLUS PLANET; EARTH-SIZED PLANET; SOLAR-TYPE STARS; SUN-LIKE STAR;
EXTRASOLAR PLANET; SPACE-TELESCOPE; HABITABLE ZONE
AB We present the characterization of the Kepler-93 exoplanetary system, based on three years of photometry gathered by the Kepler spacecraft. The duration and cadence of the Kepler observations, in tandem with the brightness of the star, enable unusually precise constraints on both the planet and its host. We conduct an asteroseismic analysis of the Kepler photometry and conclude that the star has an average density of 1.652 +/- 0.006 g cm(-3). Its mass of 0.911 +/- 0.033M(circle dot) renders it one of the lowest-mass subjects of asteroseismic study. An analysis of the transit signature produced by the planet Kepler-93b, which appears with a period of 4.72673978 +/- 9.7 x 10(-7) days, returns a consistent but less precise measurement of the stellar density, 1.72(-0.28)(+0.02) g cm(-3). The agreement of these two values lends credence to the planetary interpretation of the transit signal. The achromatic transit depth, as compared between Kepler and the Spitzer Space Telescope, supports the same conclusion. We observed seven transits of Kepler-93b with Spitzer, three of which we conducted in a new observing mode. The pointing strategy we employed to gather this subset of observations halved our uncertainty on the transit radius ratio R-P/R-star. We find, after folding together the stellar radius measurement of 0.919 +/- 0.011R(circle dot) with the transit depth, a best-fit value for the planetary radius of 1.481 +/- 0.019 R-circle plus. The uncertainty of 120 km on our measurement of the planet's size currently renders it one of the most precisely measured planetary radii outside of the solar system. Together with the radius, the planetary mass of 3.8 +/- 1.5 M-circle plus. corresponds to a rocky density of 6.3 +/- 2.6 g cm(-3). After applying a prior on the plausible maximum densities of similarly sized worlds between 1 and 1.5 R-circle plus, we find that Kepler-93b possesses an average density within this group.
C1 [Ballard, Sarah] Univ Washington, Seattle, WA 98195 USA.
[Chaplin, William J.; Davies, Guy R.; Campante, Tiago L.; Handberg, Rasmus; Elsworth, Yvonne; Hekker, Saskia] Univ Birmingham, Sch Phys & Astron, Birmingham B15 2TT, W Midlands, England.
[Chaplin, William J.; Davies, Guy R.; Aguirre, Victor Silva; Christensen-Dalsgaard, Jorgen; Metcalfe, Travis S.; Campante, Tiago L.; Handberg, Rasmus; Karoff, Christoffer; Elsworth, Yvonne; Kjeldsen, Hans; Lund, Mikkel N.; Lundkvist, Mia] Aarhus Univ, Dept Phys & Astron, Stellar Astrophys Ctr, DK-8000 Aarhus C, Denmark.
[Charbonneau, David; Fressin, Francois; Zeng, Li] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Desert, Jean-Michel] Univ Colorado, Dept Astrophys & Planetary Sci, Boulder, CO 80309 USA.
[Werner, Michael W.] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
[Basu, Sarbani] Yale Univ, Dept Astron, New Haven, CT 06520 USA.
[Metcalfe, Travis S.] Space Sci Inst, Boulder, CO 80301 USA.
[Stello, Dennis; Bedding, Timothy R.] Univ Sydney, Sch Phys, Sydney Inst Astron, Sydney, NSW 2006, Australia.
[Gilliland, Ronald L.] Penn State Univ, Ctr Exoplanets & Habitable Worlds, University Pk, PA 16802 USA.
[Hekker, Saskia] Max Planck Inst Stromungsforsch, D-37077 Gottingen, Germany.
[Hekker, Saskia] Univ Amsterdam, Astron Inst, NL-1012 WX Amsterdam, Netherlands.
[Huber, Daniel] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Huber, Daniel] SETI Inst, Mountain View, CA 94043 USA.
[Kawaler, Steven D.] Iowa State Univ, Dept Phys & Astron, Ames, IA 50011 USA.
RP Ballard, S (reprint author), Univ Washington, Seattle, WA 98195 USA.
EM sarahba@uw.edu
OI Zeng, Li/0000-0003-1957-6635; Davies, Guy/0000-0002-4290-7351; 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; Handberg, Rasmus/0000-0001-8725-4502
FU NASA through the Sagan Fellowship Program; NASA; NASA's Science Mission
Directorate; Kepler Participatory Science [NNX12AC77G, NNX09AB53G]; John
Templeton Foundation; UK Science and Technology Facilities Council
(STFC); NSF [AST-1105930]; NASA [NNX13AE70G, NNX13AE91G, NNX14AB92G];
Danish National Research Foundation [DNRF106]; ASTERISK project
(ASTERoseismic Investigations with SONG and Kepler) - European Research
Council [267864]; Netherlands Organisation for Scientific Research
(NWO); European Research Council under the European Community's Seventh
Framework Programme/ERC [338251]; Australian Research Council;
International Space Science Institute (ISSI)
FX This work was performed in part under contract with the California
Institute of Technology (Caltech) funded by NASA through the Sagan
Fellowship Program. It was conducted with observations made with the
Spitzer Space Telescope, which is operated by the Jet Propulsion
Laboratory, California Institute of Technology under a contract with
NASA. Support for this work was provided by NASA through an award issued
by JPL/Caltech. We thank the Spitzer team at the Infrared Processing and
Analysis Center in Pasadena, California, and in particular Nancy
Silbermann for scheduling the Spitzer observations of this program. This
work is also based on observations made with Kepler, which was
competitively selected as the tenth Discovery mission. Funding for this
mission is provided by NASA's Science Mission Directorate. The authors
would like to thank the many people who generously gave so much their
time to make this Mission a success. This research has 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. S. Ballard
thanks Geoffrey Marcy for helpful discussions about the RV signature of
Kepler-93. We acknowledge support through Kepler Participatory Science
Awards NNX12AC77G and NNX09AB53G, awarded to D.C. This publication was
made possible in part through the support of a grant from the John
Templeton Foundation. The opinions expressed in this publication are
those of the authors and do not necessarily reflect the views of the
John Templeton Foundation. 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). S. Basu acknowledges support from NSF grant AST-1105930
and NASA grant NNX13AE70G. Funding for the StellarAstrophysics 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). S.H.
acknowledges financial support from the Netherlands Organisation for
Scientific Research (NWO). 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. 338251 (StellarAges). T.S.M. acknowledges NASA grant
NNX13AE91G. D.S. is supported by the Australian Research Council. D.H.
acknowledges support by an appointment to the NASA Postdoctoral Program
at Ames Research Center administered by Oak Ridge Associated
Universities, and NASA grant NNX14AB92G issued through the Kepler
Participating Scientist Program. Computational time on Kraken at the
National Institute of Computational Sciences was provided through NSF
TeraGrid allocation TG-AST090107. We are also grateful for support from
the International Space Science Institute (ISSI).
NR 108
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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 JUL 20
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VL 790
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DI 10.1088/0004-637X/790/1/12
PG 16
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AL0SK
UT WOS:000338836800012
ER
PT J
AU Chung, SM
Kochanek, CS
Assef, R
Brown, MJI
Stern, D
Jannuzi, BT
Gonzalez, AH
Hickox, RC
Moustakas, J
AF Chung, Sun Mi
Kochanek, Christopher S.
Assef, Roberto
Brown, Michael J. I.
Stern, Daniel
Jannuzi, Buell T.
Gonzalez, Anthony H.
Hickox, Ryan C.
Moustakas, John
TI A UV TO MID-IR STUDY OF AGN SELECTION
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: active; galaxies: distances and redshifts; quasars: general
ID ACTIVE GALACTIC NUCLEI; DIGITAL-SKY-SURVEY; WIDE-FIELD SURVEY; QUASAR
LUMINOSITY FUNCTION; 7TH DATA RELEASE; X-RAY SURVEY; DEEP FIELD;
MIDINFRARED SELECTION; PHOTOMETRIC REDSHIFTS; BOOTES FIELD
AB We classify the spectral energy distributions (SEDs) of 431,038 sources in the 9 deg(2) Bootes field of the NOAO Deep Wide-Field Survey (NDWFS). There are up to 17 bands of data available per source, including ultraviolet (GALEX), optical (NDWFS), near-IR (NEWFIRM), and mid-infrared (IRAC and MIPS) data, as well as spectroscopic redshifts for similar to 20,000 objects, primarily from the AGN and Galaxy Evolution Survey. We fit galaxy, active galactic nucleus (AGN), stellar, and brown dwarf templates to the observed SEDs, which yield spectral classes for the Galactic sources and photometric redshifts and galaxy/AGN luminosities for the extragalactic sources. The photometric redshift precision of the galaxy and AGN samples are sigma/(1 + z) = 0.040 and sigma/(1 + z) = 0.169, respectively, with the worst 5% outliers excluded. On the basis of the chi(2)(nu) of the SED fit for each SED model, we are able to distinguish between Galactic and extragalactic sources for sources brighter than I = 23.5 mag. We compare the SED fits for a galaxy-only model and a galaxy-AGN model. Using known X-ray and spectroscopic AGN samples, we confirm that SED fitting can be successfully used as a method to identify large populations of AGNs, including spatially resolved AGNs with significant contributions from the host galaxy and objects with the emission line ratios of "composite" spectra. We also use our results to compare with the X-ray, mid-IR, optical color, and emission line ratio selection techniques. For an F-ratio threshold of F > 10, we find 16,266 AGN candidates brighter than I = 23.5 mag and a surface density of similar to 1900 AGN deg(-2).
C1 [Chung, Sun Mi; Kochanek, Christopher S.] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA.
[Assef, Roberto] Univ Diego Portales, Fac Ingn, Nucleo Astron, Santiago, Chile.
[Brown, Michael J. I.] Monash Univ, Sch Phys, Clayton, Vic 3800, Australia.
[Stern, Daniel] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Jannuzi, Buell T.] Univ Arizona, Dept Astron, Tucson, AZ 85721 USA.
[Jannuzi, Buell T.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA.
[Gonzalez, Anthony H.] Univ Florida, Dept Astron, Gainesville, FL 32611 USA.
[Hickox, Ryan C.] Dartmouth Coll, Dept Phys & Astron, Hanover, NH 03755 USA.
[Moustakas, John] Siena Coll, Dept Phys & Astron, Loudonville, NY 12211 USA.
RP Chung, SM (reprint author), Ohio State Univ, Dept Astron, 140 West 18th Ave, Columbus, OH 43210 USA.
RI Brown, Michael/B-1181-2015
OI Brown, Michael/0000-0002-1207-9137
FU Gemini-CONICYT [32120009]
FX The authors thank the Bootes collaborations for contributing to the
various Bootes photometric catalogs. The work of D.S. was carried out at
Jet Propulsion Laboratory, California Institute of Technology, under a
contract with NASA. R.J.A. was supported by Gemini-CONICYT grant number
32120009.
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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 JUL 20
PY 2014
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PG 20
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SC Astronomy & Astrophysics
GA AL0SK
UT WOS:000338836800054
ER
PT J
AU Cohen, O
Drake, JJ
Glocer, A
Garraffo, C
Poppenhaeger, K
Bell, JM
Ridley, AJ
Gombosi, TI
AF Cohen, O.
Drake, J. J.
Glocer, A.
Garraffo, C.
Poppenhaeger, K.
Bell, J. M.
Ridley, A. J.
Gombosi, T. I.
TI MAGNETOSPHERIC STRUCTURE AND ATMOSPHERIC JOULE HEATING OF HABITABLE
PLANETS ORBITING M-DWARF STARS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE magnetohydrodynamics ( MHD); planets and satellites: atmospheres;
planets and satellites: magnetic fields; planets and satellites:
terrestrial planets
ID MAIN-SEQUENCE STARS; RESISTIVE MHD SIMULATIONS; EARTH-LIKE EXOPLANETS;
EJECTION CME ACTIVITY; MASS-LOSS RATES; X-RAY-EMISSION; HOT JUPITERS;
OHMIC DISSIPATION; MAGNETIC-FIELD; HD 209458B
AB We study the magnetospheric structure and the ionospheric Joule Heating of planets orbiting M-dwarf stars in the habitable zone using a set ofmagnetohydrodynamic models. The stellarwind solution is used to drive amodel for the planetary magnetosphere, which is coupled with a model for the planetary ionosphere. Our simulations reveal that the space environment around close-in habitable planets is extreme, and the stellar wind plasma conditions change from sub-to super-Alfv ' enic along the planetary orbit. As a result, themagnetospheric structure changes dramatically with a bow shock forming in the super-Alfv ' enic sectors, while no bow shock forms in the sub-Alfv ' enic sectors. The planets reside most of the time in the sub-Alfv ' enic sectors with poor atmospheric protection. A significant amount of Joule Heating is provided at the top of the atmosphere as a result of the intense stellar wind. For the steady-state solution, the heating is about 0.1%-3% of the total incoming stellar irradiation, and it is enhanced by 50% for the time-dependent case. The significant Joule Heating obtained here should be considered in models for the atmospheres of habitable planets in terms of the thickness of the atmosphere, the top-side temperature and density, the boundary conditions for the atmospheric pressure, and particle radiation and transport. Here we assume constant ionospheric Pedersen conductance similar to that of the Earth. The conductance could be greater due to the intense EUV radiation leading to smaller heating rates. We plan to quantify the ionospheric conductance in future study.
C1 [Cohen, O.; Drake, J. J.; Garraffo, C.; Poppenhaeger, K.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Glocer, A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Bell, J. M.] Natl Inst Aerosp, Ctr Planetary Atmospheres & Flight Sci, Hampton, VA 23666 USA.
[Ridley, A. J.; Gombosi, T. I.] Univ Michigan, Ctr Space Environm Modeling, Ann Arbor, MI 48109 USA.
RP Cohen, O (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
RI Glocer, Alex/C-9512-2012; Gombosi, Tamas/G-4238-2011; Ridley,
Aaron/F-3943-2011;
OI Glocer, Alex/0000-0001-9843-9094; Gombosi, Tamas/0000-0001-9360-4951;
Ridley, Aaron/0000-0001-6933-8534; Poppenhaeger,
Katja/0000-0003-1231-2194; Cohen, Ofer/0000-0003-3721-0215
FU NASA ESS; NASA ESTO-CT; NSF KDI; DoDMURI; NASA HEC Pleiades system
[SMD-13-4076]; NASA [NAS8-03060]
FX We thank an unknown referee for comments and suggestions. The work
presented here was funded by the Smithsonian Institution Consortium for
Unlocking the Mysteries of the Universe grant " Lessons from Mars: Are
Habitable Atmospheres on Planets around M Dwarfs Viable?," and by the
Smithsonian Institute Competitive Grants Program for Science (CGPS)
grant " Can Exoplanets Around Red Dwarfs Maintain Habitable
Atmospheres?." Simulation results were obtained using the Space Weather
Modeling Framework, developed by the Center for Space Environment
Modeling, at the University of Michigan with funding support from NASA
ESS, NASA ESTO-CT, NSF KDI, and DoDMURI. The simulations were performed
on the NASA HEC Pleiades system under award SMD-13-4076. J. J. D. was
supported by NASA contract NAS8-03060 to the Chandra X-ray Center during
the course of this research and thanks the Director, H. Tananbaum, for
continuing support and encouragement.
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
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J9 ASTROPHYS J
JI Astrophys. J.
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SC Astronomy & Astrophysics
GA AL0SK
UT WOS:000338836800057
ER
EF