FN Thomson Reuters Web of Science™ VR 1.0 PT J AU Romano, P Sidoli, L Cusumano, G Evans, PA Ducci, L Krimm, HA Vercellone, S Page, KL Beardmore, AP Burrows, DN Kennea, JA Gehrels, N La Parola, V Mangano, V AF Romano, P. Sidoli, L. Cusumano, G. Evans, P. A. Ducci, L. Krimm, H. A. Vercellone, S. Page, K. L. Beardmore, A. P. Burrows, D. N. Kennea, J. A. Gehrels, N. La Parola, V. Mangano, V. TI Multiple flaring activity in the supergiant fast X-ray transient IGR J08408-4503 observed with Swift SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE X-rays: individual: IGR J08408-4503 ID CLUMPY STELLAR WINDS; NEUTRON-STAR; OUTBURST AB IGR J08408-4503 is a supergiant fast X-ray transient discovered in 2006 with a confirmed association with a O8.5Ib(f) supergiant star, HD 74194. We report on the analysis of two outbursts caught by Swift/Burst Alert Telescope (BAT) on 2006 October 4 and 2008 July 5, and followed up at softer energies with Swift/X-ray Telescope (XRT). The 2008 XRT light curve shows a multiple-peaked structure with an initial bright flare that reached a flux of similar to 10(-9) erg cm(-2) s(-1) (2-10 keV), followed by two equally bright flares within 75 ks. The spectral characteristics of the flares differ dramatically, with most of the difference, as derived via time-resolved spectroscopy, being due to absorbing column variations. We observe a gradual decrease in the N(H), derived with a fit using absorbed power-law model, as time passes. We interpret these NH variations as due to an ionization effect produced by the first flare, resulting in a significant decrease in the measured column density towards the source. The durations of the flares as well as the times of the outbursts suggest that the orbital period is similar to 35 d, if the flaring activity is interpreted within the framework of the Sidoli et al. model with the outbursts triggered by the neutron star passage inside an equatorial wind inclined with respect to the orbital plane. C1 [Romano, P.; Cusumano, G.; La Parola, V.; Mangano, V.] Ist Astrofis Spaziale & Fis Cosm, INAF, I-90146 Palermo, Italy. [Sidoli, L.; Ducci, L.; Vercellone, S.] Ist Astrofis Spaziale & Fis Cosm, INAF, I-20133 Milan, Italy. [Evans, P. A.; Page, K. L.; Beardmore, A. P.] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England. [Ducci, L.] Univ Insubria, Dipartimento Matemat & Fis, I-22100 Como, Italy. [Krimm, H. A.] Univ Space Res Assoc, Columbia, MD USA. [Krimm, H. A.; Gehrels, N.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Burrows, D. N.; Kennea, J. A.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. RP Romano, P (reprint author), Ist Astrofis Spaziale & Fis Cosm, INAF, Via U La Malfa 153, I-90146 Palermo, Italy. EM romano@ifc.inaf.it RI Gehrels, Neil/D-2971-2012; OI Cusumano, Giancarlo/0000-0002-8151-1990; Sidoli, Lara/0000-0001-9705-2883; Vercellone, Stefano/0000-0003-1163-1396; La Parola, Valentina/0000-0002-8087-6488 FU Italy [ASI/INAFI/088/06/0, I/023/05/0]; Swift project; NASA [NAS5-00136] FX We thank the Swift team for making these observations possible, the duty scientists and science planners. We also thank the anonymous referee for comments that helped improve the paper. This work was supported in Italy by contracts ASI/INAFI/088/06/0 and I/023/05/0. APB, PAE and KLP acknowledge STFC support. HAK was supported by the Swift project. DNB and JAK acknowledge support from NASA contract NAS5-00136. NR 33 TC 18 Z9 18 U1 0 U2 0 PU WILEY-BLACKWELL PUBLISHING, INC PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD JAN 1 PY 2009 VL 392 IS 1 BP 45 EP 51 DI 10.1111/j.1365-2966.2008.14050.x PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 392KX UT WOS:000262302700004 ER PT J AU De Pasquale, M Evans, P Oates, S Page, M Zane, S Schady, P Breeveld, A Holland, S Kuin, P Still, M Roming, P Ward, P AF De Pasquale, M. Evans, P. Oates, S. Page, M. Zane, S. Schady, P. Breeveld, A. Holland, S. Kuin, P. Still, M. Roming, P. Ward, P. TI Jet breaks at the end of the slow decline phase of Swift GRB light curves SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE gamma-rays: bursts ID GAMMA-RAY BURSTS; THEORETICAL IMPLICATIONS; AFTERGLOW EMISSION; ENERGY RESERVOIR; FIREBALL MODEL; TELESCOPE; LONG; CALIBRATION; REDSHIFT AB The Swift mission has discovered an intriguing feature of gamma-ray burst (GRBs) afterglows, a phase of shallow decline of the flux in the X-ray and optical light curves. This behaviour is typically attributed to energy injection into the burst ejecta. At some point this phase ends, resulting in a break in the light curve, which is commonly interpreted as the cessation of the energy injection. In a few cases, however, while breaks in the X-ray light curve are observed, optical emission continues its slow flux decline. This behaviour suggests a more complex scenario. In this paper, we present a model that invokes a double component outflow, in which narrowly collimated ejecta are responsible for the X-ray emission while a broad outflow is responsible for the optical emission. The narrow component can produce a jet break in the X-ray light curve at relatively early times, while the optical emission does not break due to its lower degree of collimation. In our model both components are subject to energy injection for the whole duration of the follow-up observations. We apply this model to GRBs with chromatic breaks, and we show how it might change the interpretation of the GRBs canonical light curve. We also study our model from a theoretical point of view, investigating the possible configurations of frequencies and the values of GRB physical parameters allowed in our model. C1 [De Pasquale, M.; Oates, S.; Page, M.; Zane, S.; Schady, P.; Breeveld, A.; Kuin, P.; Still, M.; Ward, P.] Univ Coll London, Mullard Space Sci Lab, Dorking RH5 6NT, Surrey, England. [Evans, P.] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England. [Holland, S.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Roming, P.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. RP De Pasquale, M (reprint author), Univ Coll London, Mullard Space Sci Lab, Holmbury St Mary, Dorking RH5 6NT, Surrey, England. EM mdp@mssl.ucl.ac.uk NR 55 TC 20 Z9 20 U1 0 U2 1 PU WILEY-BLACKWELL PUBLISHING, INC PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD JAN 1 PY 2009 VL 392 IS 1 BP 153 EP 169 DI 10.1111/j.1365-2966.2008.13990.x PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 392KX UT WOS:000262302700009 ER PT J AU Schurch, MPE Coe, MJ Galache, JL Corbet, RHD McGowan, KE McBride, VA Townsend, LJ Udalski, A Haberl, F AF Schurch, M. P. E. Coe, M. J. Galache, J. L. Corbet, R. H. D. McGowan, K. E. McBride, V. A. Townsend, L. J. Udalski, A. Haberl, F. TI High-mass X-ray binary SXP18.3 undergoes the longest type II outburst ever seen in the Small Magellanic Cloud SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE stars: emission-line, Be; Magellanic Clouds; X-rays: binaries ID GRAVITATIONAL LENSING EXPERIMENT; PULSARS; CATALOG; SYSTEM AB On 2006 August 30, SXP18.3 a high-mass X-ray binary (HMXB) in the Small Magellanic Cloud (SMC) with an 18.3 s pulse period was observed by Rossi X-ray Timing Explorer (RXTE). The source was seen continuously for the following 36 weeks. This is the longest type II outburst ever seen from a HMXB in the SMC. During the outburst, SXP18.3 was located from serendipitous XMM-Newton observations. The identification of the optical counterpart has allowed SXP18.3 to be classified as a Be/X-ray binary. This paper will report on the analysis of the optical and weekly RXTE X-ray data that span the last 10 yr. The extreme length of this outburst has for the first time enabled us to perform an extensive study of the pulse timing of a SMC Be/X-ray binary. We present a possible full orbital solution from the pulse timing data. An orbital period of 17.79 d is proposed from the analysis of the Optical Gravitational Lensing Experiment (OGLE) III light curve placing SXP18.3 on the boundary of known sources in the Corbet diagram. C1 [Schurch, M. P. E.; Coe, M. J.; McGowan, K. E.; McBride, V. A.; Townsend, L. J.] Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England. [Galache, J. L.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Corbet, R. H. D.] Univ Maryland Baltimore Cty, Xray Astrophys Lab, NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Udalski, A.] Univ Warsaw Observ, PL-00478 Warsaw, Poland. RP Schurch, MPE (reprint author), Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England. EM mpes@astro.soton.ac.uk OI Haberl, Frank/0000-0002-0107-5237 FU National Aeronautics and Space Administration; National Science Foundation; Polish MNiSW [N20303032/4275] FX This publication makes use of data products from the Two-Micron All-Sky Survey (2MASS), which is a joint project of the University of Massachusetts and the Infrared Processing and Analysis Center/California Institute of Technology, funded by the National Aeronautics and Space Administration and the National Science Foundation. This paper utilizes public domain data originally obtained by the MACHO Project, whose work was performed under the joint auspices of the US Department of Energy, National Nuclear Security Administration by the University of California, Lawrence Livermore National Laboratory under contract number W-7405-Eng- 48, the National Science Foundation through the Center for Particle Astrophysics of the University of California under cooperative agreement AST-8809616 and the Mount Stromlo and Siding Spring Observatory, part of the Australian National University. This research has made use of the SIMBAD data base, operated by CDS, Strasbourg, France. We acknowledge support from the NASA Swift team in providing ToO observations in order to locate the source. The OGLE project is partially supported by the Polish MNiSW grant N20303032/4275. NR 30 TC 9 Z9 9 U1 0 U2 0 PU WILEY-BLACKWELL PUBLISHING, INC PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD JAN 1 PY 2009 VL 392 IS 1 BP 361 EP 366 DI 10.1111/j.1365-2966.2008.14048.x PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 392KX UT WOS:000262302700027 ER PT J AU Xu, KM AF Xu, Kuan-Man TI Evaluation of Cloud Physical Properties of ECMWF Analysis and Re-Analysis (ERA) against CERES Tropical Deep Convective Cloud Object Observations SO MONTHLY WEATHER REVIEW LA English DT Article ID LARGE-SCALE MODELS; 1998 EL-NINO; STATISTICAL-ANALYSES; DIURNAL CYCLE; PART I; SATELLITE; SCHEME; VALIDATION; CLIMATE; SURFACE AB This study presents an approach that converts the vertical profiles of grid-averaged cloud properties from large-scale models to probability density functions (pdfs) of subgrid-cell cloud physical properties measured at satellite footprints. Cloud physical and radiative properties, rather than just cloud and precipitation occurrences, of assimilated cloud systems by the European Centre for Medium-Range Weather Forecasts (ECMWF) operational analysis (EOA) and 40-yr ECMWF Re-Analysis (ERA-40) are validated against those obtained from Earth Observing System satellite cloud object data for the January-August 1998 and March 2000 periods. These properties include the ice water path (IWP), cloud-top height and temperature, cloud optical depth, and solar and infrared radiative fluxes. Each cloud object, a contiguous region with similar cloud physical properties, is temporally and spatially matched with EOA and ERA-40 data. Results indicate that most pdfs of EOA and ERA-40 cloud physical and radiative properties agree with those of satellite observations of the tropical deep convective cloud object type for the January-August 1998 period. There are, however, significant discrepancies in selected ranges of the cloud property pdfs such as the upper range of EOA cloud-top height. A major discrepancy is that the dependence of the pdfs on the cloud object size for both EOA and ERA-40 is not as strong as in the observations. Modifications to the cloud parameterization in ECMWF that occurred in October 1999 eliminate the clouds near the tropopause but shift power of the pdf to lower cloud-top heights and greatly reduce the ranges of IWP and cloud optical depth pdfs. These features persist in ERA-40 due to the use of the same cloud parameterizations. The less sophisticated data assimilation technique and the lack of snow water content information in ERA-40, not the larger horizontal grid spacing, are also responsible for the disagreements with observed pdfs of cloud physical properties, although the detection rates of cloud object occurrence are improved for small-size categories. A possible improvement to the convective parameterization is to introduce a stronger dependence of updraft penetration heights on grid-cell dynamics. C1 NASA, Langley Res Ctr, Climate Sci Branch, Hampton, VA 23681 USA. RP Xu, KM (reprint author), NASA, Langley Res Ctr, Climate Sci Branch, Mail Stop 420, Hampton, VA 23681 USA. EM Kuan-Man.Xu@nasa.gov RI Xu, Kuan-Man/B-7557-2013 OI Xu, Kuan-Man/0000-0001-7851-2629 FU NASA FX The CERES data were obtained from the Atmospheric Sciences Data Center at the NASA Langley Research Center. This research has been supported by the NASA modeling, analysis, and prediction program and interdisciplinary study program ( Drs. D. Anderson and H. Maring, program managers). The author would like to thank Dr. Takmeng Wong, Mr. Lindsay Parker, and Ms. Shengtao Dong for producing the cloud object data and the matched ECMWF data. Discussions with Drs. Bruce Wielicki, Takmeng Wong, and Zachary Eitzen are very helpful. Comments from Drs. Martin Kuhler and Peter Bechtold of ECMWF and two anonymous reviewers are greatly appreciated. NR 60 TC 7 Z9 7 U1 0 U2 5 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 0027-0644 J9 MON WEATHER REV JI Mon. Weather Rev. PD JAN PY 2009 VL 137 IS 1 BP 207 EP 223 DI 10.1175/2008MWR2633.1 PG 17 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 404VU UT WOS:000263181900012 ER PT J AU Vj, L Kobayashi, NP Islam, MS Wu, W Chaturvedi, P Fang, NX Wang, SY Williams, RS AF Vj, Logeeswaran Kobayashi, Nobuhiko P. Islam, M. Saif Wu, Wei Chaturvedi, Pratik Fang, Nicholas X. Wang, Shih Yuan Williams, R. Stanley TI Ultrasmooth Silver Thin Films Deposited with a Germanium Nucleation Layer SO NANO LETTERS LA English DT Article ID AG FILMS; MORPHOLOGY; GROWTH; INTERFACE; DIFFUSION; SURFACES; GOLD; SIO2 AB We demonstrate an effective method for depositing smooth silver (Ag) films on SiO/Si-2(100) substrates using a thin seed layer of evaporated germanium (Ge). The deposited Ag films exhibit smaller root-mean-square surface roughness, narrower peak-to-valley surface topological height distribution, smaller grain-size distribution, and smaller sheet resistance in comparison to those of Ag films directly deposited on SiO2/Si(100) substrates. Optically thin (similar to 10-20 nm) Ag films deposited with similar to 1-2 nm Ge nucleation layers show more than an order of magnitude improvement in the surface roughness. The presence of the thin layer of Ge changes the growth kinetics (nucleation and evolution) of the electron-beam-evaporated Ag, leading to Ag films with smooth surface morphology and high electrical conductivity. The demonstrated Ag thin films are very promising for large-scale applications as molecular anchors, optical metamaterials, plasmonic devices, and several areas of nanophotonics. C1 [Vj, Logeeswaran; Islam, M. Saif] Univ Calif Davis, Dept Elect & Comp Engn, Davis, CA 95616 USA. [Wu, Wei; Wang, Shih Yuan; Williams, R. Stanley] Hewlett Packard Labs, Informat & Quantum Syst Labs, Palo Alto, CA 94304 USA. [Chaturvedi, Pratik; Fang, Nicholas X.] Univ Illinois, Dept Engn Sci & Mech, Urbana, IL 61801 USA. [Kobayashi, Nobuhiko P.] Univ Calif Santa Cruz, Jack Baskin Sch Engn, Santa Cruz, CA 95064 USA. [Kobayashi, Nobuhiko P.] Univ Calif Santa Cruz, NECTAR, Adv Studies Labs, Santa Cruz, CA 95064 USA. [Kobayashi, Nobuhiko P.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Islam, MS (reprint author), Univ Calif Davis, Dept Elect & Comp Engn, Kemper Hall,1 Shields Ave, Davis, CA 95616 USA. EM sislam@ucdavis.edu RI Fang, Nicholas/A-5856-2008; Wang, Shih-Yuan/C-3889-2009; Chaturvedi, Pratik/A-8922-2010; Wu, Wei/D-1908-2011; Williams, R. Stanley/A-8281-2009; Kobayashi, Nobuhiko/E-3834-2012 OI Fang, Nicholas/0000-0001-5713-629X; Wang, Shih-Yuan/0000-0002-1212-3484; Williams, R. Stanley/0000-0003-0213-4259; FU Information and Quantum Systems Laboratories in Hewlett-Packard Laboratories, Palo Alto CA; NSF [0547679]; UC Davis FX The authors thank Zhiyong Li, Sagi Mathai, Xuema Li, Doug Ohlberg, William Tong, and Denny Houng of Information and Quantum Systems Laboratories in Hewlett-Packard Laboratories, Palo Alto CA, David A. Horsley, Chan Mei-Lin, and Jack Skinner of UC DavisBerkeley Sensor & Actuator Center, and A. Alec Talin from Sandia National Laboratories-Livermore for valuable discussions. The work at UC Davis was partially supported by NSF Grant #0547679 and a UC Davis research grant. NR 34 TC 34 Z9 34 U1 5 U2 44 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 1530-6984 EI 1530-6992 J9 NANO LETT JI Nano Lett. PD JAN PY 2009 VL 9 IS 1 BP 178 EP 182 DI 10.1021/nl8027476 PG 5 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 395IZ UT WOS:000262519100033 ER PT J AU Whitelam, S Rogers, C Pasqua, A Paavola, C Trent, J Geissler, PL AF Whitelam, Stephen Rogers, Carl Pasqua, Andrea Paavola, Chad Trent, Jonathan Geissler, Phillip L. TI The Impact of Conformational Fluctuations on Self-Assembly: Cooperative Aggregation of Archaeal Chaperonin Proteins SO NANO LETTERS LA English DT Article ID SULFOLOBUS-SHIBATAE; BUILDING-BLOCKS; DYNAMICS AB Protein complexes called rosettasomes self-assemble in solution to form large-scale filamentous and planar structures. The relative abundance of these aggregates varies abruptly with environmental conditions and sample composition. Our simulations of a model of patchy nanoparticles can reproduce this sharp crossover, but only if particles are allowed to switch between two internal states favoring different geometries of local binding. These results demonstrate how local conformational adaptivity can fundamentally influence the cooperativity of pattern-forming dynamics. C1 [Pasqua, Andrea; Geissler, Phillip L.] Univ Calif Berkeley, Dept Chem, Berkeley, CA 94720 USA. [Whitelam, Stephen] Univ Warwick, Syst Biol Ctr, Coventry CV4 7AL, W Midlands, England. [Rogers, Carl] Univ Calif Berkeley, Biophys Grad Grp, Berkeley, CA 94720 USA. [Paavola, Chad; Trent, Jonathan] NASA, Ames Res Ctr, Bioengn Branch, Moffett Field, CA 94305 USA. [Geissler, Phillip L.] Lawrence Berkeley Natl Lab, Div Mat Sci, Berkeley, CA 94720 USA. [Geissler, Phillip L.] Lawrence Berkeley Natl Lab, Div Phys Biosci, Berkeley, CA 94720 USA. [Geissler, Phillip L.] Lawrence Berkeley Natl Lab, Div Chem Sci, Berkeley, CA 94720 USA. RP Geissler, PL (reprint author), Univ Calif Berkeley, Dept Chem, Berkeley, CA 94720 USA. EM geissler@berkeley.edu FU U.S. Department of Energy [DE-AC02-05CH11231]; BioSim European Union Network of Excellence [LSHB-CT-2004-005137]; NIH Molecular Biophysics Training [T32GM08295]; Science Research Investment Fund FX This work was supported by the Director, Office of Science, Office of Basic Energy Sciences, Materials Sciences and Engineering Division, of the U.S. Department of Energy under Contract No. DE-AC02-05CH11231. S.W. was supported by the BioSim European Union Network of Excellence (LSHB-CT-2004-005137). C.R. was supported by a NIH Molecular Biophysics Training Grant (T32GM08295). Computing facilities were provided in part by the Centre for Scientific Computing at the University of Warwick with support from the Science Research Investment Fund. We used VMD22 to render simulation configurations. NR 22 TC 15 Z9 15 U1 0 U2 12 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 1530-6984 J9 NANO LETT JI Nano Lett. PD JAN PY 2009 VL 9 IS 1 BP 292 EP 297 DI 10.1021/nl8029306 PG 6 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 395IZ UT WOS:000262519100055 PM 19072304 ER PT S AU Andrews, RJ AF Andrews, Russell J. BE Sharma, HS TI Neuromodulation: deep brain stimulation, sensory neuroprostheses, and the neural-electrical interface SO NANONEUROSCIENCE AND NANONEUROPHARMACOLOGY SE Progress in Brain Research LA English DT Review; Book Chapter DE brainstem implants; carbon nanotubes; cochlear implants; computational analysis; deep brain stimulation; nanoelectrode arrays; neural-electrical interface; neuromodulation; retinal implants; sensory neuroprostheses ID SUBTHALAMIC NUCLEUS; PARKINSONS-DISEASE; RELEASE; SYSTEM; PERFORMANCE; PROSTHESIS; ASTROCYTES; IMPLANT; NEURONS; HEARING AB Although neuromodulation with implanted brain electrodes (deep brain stimulation, DBS) has been increasingly effective in treating many patients with movement disorders (e.g., advanced Parkinson's disease) over the past 20 years, the techniques have changed little for more than 50 years. After summarizing the current state of DBS, this chapter considers (1) the advances being offered by computational analysis techniques as well as (2) the benefits of monitoring and modulating brain chemical activity in addition to brain electrical activity. A review of the current state of sensory neuroprostheses follows, with consideration of emerging data on the optimal configuration of micron-sized retinal prostheses as well as on the optimal site for stimulation of cells in the retina. Very recent findings on nanotechniques to enhance charge transfer from prosthesis to cell (neuronal or glial), that is, enhancement of the neural-electrical interface, are then reviewed. The final section summarizes areas of potential cross-fertilization between those centers developing sensory neuroprostheses and those centers developing nanotechniques for DBS. C1 NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Andrews, RJ (reprint author), NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. EM rja@russelljandrews.org NR 28 TC 2 Z9 2 U1 2 U2 10 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA SARA BURGERHARTSTRAAT 25, PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0079-6123 BN 978-0-444-53431-6 J9 PROG BRAIN RES JI Prog. Brain Res. PY 2009 VL 180 BP 127 EP 139 DI 10.1016/S0079-6123(08)80007-6 PG 13 WC Nanoscience & Nanotechnology; Neurosciences SC Science & Technology - Other Topics; Neurosciences & Neurology GA BQC14 UT WOS:000280620600008 PM 20302832 ER PT S AU Son, KA Yang, BH Prokopuk, N Moon, JS Liao, A Gallegos, M Yang, JW Katona, T Khan, MA AF Son, K. -A. Yang, B. H. Prokopuk, N. Moon, J. S. Liao, A. Gallegos, M. Yang, J. W. Katona, T. Khan, M. A. BE Nagarajan, R Zukas, W Hatton, TA Lee, S TI Novel GaN-based Chemical Sensors for Long-range Chemical Threat Detection SO NANOSCIENCE AND NANOTECHNOLOGY FOR CHEMICAL AND BIOLOGICAL DEFENSE SE ACS Symposium Series LA English DT Proceedings Paper CT 234th American-Chemical-Society National Meeting CY AUG 17-19, 2007 CL Boston, MA SP Amer Chem Soc, Div Colloid & Surface Chem ID ELECTRON-MOBILITY-TRANSISTORS; FIELD-EFFECT TRANSISTORS; PIEZOELECTRIC POLARIZATION; ALGAN/GAN HETEROSTRUCTURES; SF6 AB We are developing micro chemical sensor nodes consisting of GaN HEMT (High Electron Mobility Transistor) sensors and a RF communication link for long range chemical threat detection and early warning. In this paper, we discuss our research on (1) high selectivity detection of chemical agents (stimulants) using the GaN HEMT sensors, (2) the effects of the materials and design of the gate electrode on the sensitivity of the sensor, and (3) optimal operating parameters for high sensitivity detection. C1 [Son, K. -A.; Yang, B. H.; Liao, A.; Gallegos, M.] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. RP Son, KA (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. NR 18 TC 0 Z9 0 U1 1 U2 2 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 SIXTEENTH ST NW, WASHINGTON, DC 20036 USA SN 0097-6156 BN 978-0-8412-6981-1 J9 ACS SYM SER JI ACS Symp. Ser. PY 2009 VL 1016 BP 155 EP 168 PG 14 WC Biochemistry & Molecular Biology; Chemistry, Multidisciplinary; Nanoscience & Nanotechnology SC Biochemistry & Molecular Biology; Chemistry; Science & Technology - Other Topics GA BVW58 UT WOS:000292990100012 ER PT B AU Vasquez, A Ewert, M Rowlands, J Post, K AF Vasquez, A. Ewert, M. Rowlands, J. Post, K. BE Laudon, M Romanowicz, B TI Johnson Space Center's Solar and Wind-based Renewable Energy System SO NANOTECH CONFERENCE & EXPO 2009, VOL 3, TECHNICAL PROCEEDINGS LA English DT Proceedings Paper CT Nanotech 2009 Conference CY MAY 03-07, 2009 CL Houston, TX SP Acctron AG, Adv Energy Consortium, Alliance NanoHealth, Appl Mat, Bayer MaterialScience, Buchanan Ingersoll & Rooney PC, Buhler PARTEC GmbH, Ctr Appl Nanotechnol GmbH, Ctr Biol & Environm Nanotechnol, Clean Technol & Sustainable Ind Org, CMP, CTC Nanotechnol GmbH, DREEBIT GmbH, ETH Zurich, ETH Transfer, ETH Zurich, MNSP, Folcy & Lardner LLP, FDA, Goodwin Procter LLC, HiNanoAnalytics, Houston Technol Ctr, Inno X GmbH, Innovat Alliance Carbon Nanotubes, Italian Tradde Commiss, Jackson Walket LLP, JENOPTIK, Lockheed Martin, Nano Sci & Technol Inst, nano tech 2009 Japan, NanoEurope Fair & Conf, Nanograde Llc, NanoInk, NANOSENSORS, NanoSPRINT, NanoWorld AG, NCI, NIH, Opportun Houston, OSEC, Pearland Econ Dev Corp, Res Germany Land Ideas, Richard Smalley Inst Nanoscale Sci & Technol, Taylor & Francis Grp LLC, CRC Press, TechConnect, Texas Nanotechnol Initiat, IEEE Stand Assoc, Russian Corp Nanotechnologies, TurboBeads Llc, Weidmann Plast Technol AG DE renewable-energy; solar; photovoltaic; wind-turbine; space-exploration power AB The NASA Johnson Space Center (JSC) in Houston, Texas has a Sustainability Partnership team that seeks ways for earth-based sustainability practices to also benefit space exploration research. A renewable energy gathering system was installed in 2007 at the JSC Child Care Center (CCC) which also offers a potential test bed for space exploration power generation and remote monitoring and control concepts. The system comprises: 1) several different types of photovoltaic panels (29 M), 2) two wind-turbines (3.6 kW total), and 3) one roof-mounted solar thermal water heater and tank. A tie to the JSC local electrical grid was provided to accommodate excess power. The total first year electrical energy production was 53 megawatt-hours. A web-based real-time metering system collects and reports system performance and weather data. Improvements in areas of the CCC that were detected during subsequent energy analyses and some concepts for future efforts are also presented. C1 [Vasquez, A.; Ewert, M.; Rowlands, J.; Post, K.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. RP Vasquez, A (reprint author), NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. EM Arturo.Vasquez-1@nasa.gov; Michael.K.Ewert@nasa.gov; Jerald.T.Rowlands@nasa.gov; Kevin.E.Post@nasa.gov NR 1 TC 0 Z9 0 U1 0 U2 0 PU CRC PRESS-TAYLOR & FRANCIS GROUP PI BOCA RATON PA 6000 BROKEN SOUND PARKWAY NW, STE 300, BOCA RATON, FL 33487-2742 USA BN 978-1-4398-1784-1 PY 2009 BP 137 EP 140 PG 4 WC Energy & Fuels; Nanoscience & Nanotechnology SC Energy & Fuels; Science & Technology - Other Topics GA BMQ04 UT WOS:000273331000033 ER PT B AU Wilson, WC Atkinson, GM AF Wilson, W. C. Atkinson, G. M. BE Laudon, M Romanowicz, B TI A Comparison of Surface Acoustic Wave Modeling Methods SO NANOTECH CONFERENCE & EXPO 2009, VOL 3, TECHNICAL PROCEEDINGS LA English DT Proceedings Paper CT Nanotech 2009 Conference CY MAY 03-07, 2009 CL Houston, TX SP Acctron AG, Adv Energy Consortium, Alliance NanoHealth, Appl Mat, Bayer MaterialScience, Buchanan Ingersoll & Rooney PC, Buhler PARTEC GmbH, Ctr Appl Nanotechnol GmbH, Ctr Biol & Environm Nanotechnol, Clean Technol & Sustainable Ind Org, CMP, CTC Nanotechnol GmbH, DREEBIT GmbH, ETH Zurich, ETH Transfer, ETH Zurich, MNSP, Folcy & Lardner LLP, FDA, Goodwin Procter LLC, HiNanoAnalytics, Houston Technol Ctr, Inno X GmbH, Innovat Alliance Carbon Nanotubes, Italian Tradde Commiss, Jackson Walket LLP, JENOPTIK, Lockheed Martin, Nano Sci & Technol Inst, nano tech 2009 Japan, NanoEurope Fair & Conf, Nanograde Llc, NanoInk, NANOSENSORS, NanoSPRINT, NanoWorld AG, NCI, NIH, Opportun Houston, OSEC, Pearland Econ Dev Corp, Res Germany Land Ideas, Richard Smalley Inst Nanoscale Sci & Technol, Taylor & Francis Grp LLC, CRC Press, TechConnect, Texas Nanotechnol Initiat, IEEE Stand Assoc, Russian Corp Nanotechnologies, TurboBeads Llc, Weidmann Plast Technol AG DE Surface Acoustic Wave; SAW; transmission line models; Impulse Response Method AB Surface Acoustic Wave (SAW) technology is low cost, rugged, lightweight, extremely low power and call be used to develop passive wireless sensors. For these reasons, NASA is investigating the use of SAW technology for Integrated Vehicle Health Monitoring (IVHM) of aerospace structures. To facilitate rapid prototyping of passive SAW sensors for aerospace applications,, SAW models have been developed. This paper reports oil the comparison of three methods of modeling SAWs. The three models are the Impulse Response Method a first order model, and two second order matrix methods; the conventional matrix approach, and a modified matrix approach that is extended to include internal finger reflections. The second order models are based upon matrices that were originally developed for analyzing microwave circuits using transmission line theory. Results from the models are presented with measured data from devices. C1 [Wilson, W. C.] NASA, Langley Res Ctr, Hampton, VA 23665 USA. RP Wilson, WC (reprint author), NASA, Langley Res Ctr, Hampton, VA 23665 USA. EM w.c.wilson@larc.nasa.gov; gmatkins@vcu.edu NR 4 TC 1 Z9 1 U1 0 U2 0 PU CRC PRESS-TAYLOR & FRANCIS GROUP PI BOCA RATON PA 6000 BROKEN SOUND PARKWAY NW, STE 300, BOCA RATON, FL 33487-2742 USA BN 978-1-4398-1784-1 PY 2009 BP 347 EP 350 PG 4 WC Energy & Fuels; Nanoscience & Nanotechnology SC Energy & Fuels; Science & Technology - Other Topics GA BMQ04 UT WOS:000273331000088 ER PT J AU Bleier, T Dunson, C Maniscalco, M Bryant, N Bambery, R Freund, F AF Bleier, T. Dunson, C. Maniscalco, M. Bryant, N. Bambery, R. Freund, F. TI Investigation of ULF magnetic pulsations, air conductivity changes, and infra red signatures associated with the 30 October Alum Rock M5.4 earthquake SO NATURAL HAZARDS AND EARTH SYSTEM SCIENCES LA English DT Article ID CHI-CHI EARTHQUAKE; ELECTRIC-CURRENTS; CALIFORNIA; SIGNALS AB Several electromagnetic signal types were observed prior to and immediately after 30 October 2007 (Local Time) M5.4 earthquake at Alum Rock, Ca with an epicenter similar to 15 km NE of San Jose Ca. The area where this event occurred had been monitored since November 2005 by a QuakeFinder magnetometer site, unit 609, 2 km from the epicenter. This instrument is one of 53 stations of the QuakeFinder (QF) California Magnetometer Network-CalMagNet. This station included an ultra low frequency (ULF) 3-axis induction magnetometer, a simple air conductivity sensor to measure relative airborne ion concentrations, and a geophone to identify the arrival of the P-wave from an earthquake. Similar in frequency content to the increased ULF activity reported two weeks prior to the Loma Prieta M7.0 quake in 1989 (Fraser-Smith, 1990, 1991), the QF station detected activity in the 0.01-12 Hz bands, but it consisted of an increasing number of short duration (1 to 30 s duration) pulsations. The pulsations peaked around 13 days prior to the event. The amplitudes of the pulses were strong, (3-20 nT), compared to the average ambient noise at the site, (10-250 pT), which included a component arising from the Bay Area Rapid Transit (BART) operations. The QF station also detected different pulse shapes, e. g. negative or positive only polarity, with some pulses including a combination of positive and negative. Typical pulse counts over the previous year ranged from 0-15 per day, while the count rose to 176 (east-west channel) on 17 October, 13 days prior to the quake. The air conductivity sensor saturated for over 14 h during the night and morning prior to the quake, which occurred at 20: 29 LT. Anomalous IR signatures were also observed in the general area, within 50 km of the epicenter, during the 2 weeks prior to the quake. These three simultaneous EM phenomena were compared with data collected over a 1-2-year period at the site. The data was also compared against accounts of air ionization reported to be associated with radon emission from the ground (Ouzounov, 2007), and a series of laboratory rock stressing experiments (Freund, 2006, 2007a, b, c) to determine if field data was consistent either of these accounts. We could not find a data set with pre-earthquake radon measurements taken near the Alum Rock epicenter to compare against our field data. However, based on the Alum Rock data set example and another data set at Parkfield, the field tests are at least consistent with the lab experiments showing currents, magnetic field disturbances, air conductivity changes, and IR signatures. This is encouraging, but more instrumented earthquake examples are needed to prove a repeating pattern for these types of pre-earthquake EM signatures. C1 [Bleier, T.; Dunson, C.; Maniscalco, M.] QuakeFinder Inc, Palo Alto, CA 94306 USA. [Bryant, N.; Bambery, R.] NASA, Jet Prop Lab, Pasadena, CA 91109 USA. [Freund, F.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Bleier, T (reprint author), QuakeFinder Inc, Palo Alto, CA 94306 USA. EM tbleier@quakefinder.com NR 19 TC 28 Z9 28 U1 0 U2 6 PU COPERNICUS PUBLICATIONS PI KATHLENBURG-LINDAU PA MAX-PLANCK-STR 13, KATHLENBURG-LINDAU, 37191, GERMANY SN 1561-8633 J9 NAT HAZARD EARTH SYS JI Nat. Hazards Earth Syst. Sci. PY 2009 VL 9 IS 2 BP 585 EP 603 PG 19 WC Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences; Water Resources SC Geology; Meteorology & Atmospheric Sciences; Water Resources GA 441BD UT WOS:000265743400026 ER PT J AU Kirschbaum, DB Adler, R Hong, Y Lerner-Lam, A AF Kirschbaum, D. B. Adler, R. Hong, Y. Lerner-Lam, A. TI Evaluation of a preliminary satellite-based landslide hazard algorithm using global landslide inventories SO NATURAL HAZARDS AND EARTH SYSTEM SCIENCES LA English DT Article ID DEBRIS FLOWS; SHALLOW LANDSLIDES; RAINFALL INTENSITY; DURATION CONTROL; CENTRAL NEPAL; HONG-KONG; SUSCEPTIBILITY; GIS; PRODUCTS; MONSOON AB Most landslide hazard assessment algorithms in common use are applied to small regions, where high-resolution, in situ, observables are available. A preliminary global landslide hazard algorithm has been developed to estimate areas of potential landslide occurrence in near real-time by combining a calculation of landslide susceptibility with satellite derived rainfall estimates to forecast areas with increased potential for landslide conditions. This paper presents a stochastic methodology to compare this new, landslide hazard algorithm for rainfall-triggered landslides with a newly available inventory of global landslide events, in order to determine the predictive skill and limitations of such a global estimation technique. Additionally, we test the sensitivity of the global algorithm to its input observables, including precipitation, topography, land cover and soil variables. Our analysis indicates that the current algorithm is limited by issues related to both the surface-based susceptibility map and the temporal resolution of rainfall information, but shows skill in determining general geographic and seasonal distributions of landslides. We find that the global susceptibility model has inadequate performance in certain locations, due to improper weighting of surface observables in the susceptibility map. This suggests that the relative contributions of topographic slope and soil conditions to landslide susceptibility must be considered regionally. The current, initial forecast system, although showing some overall skill, must be improved considerably if it is to be used for hazard warning or detailed studies. Surface and remote sensing observations at higher spatial resolution, together with improved landslide event catalogues, are required if global landslide hazard forecasts are to become an operational reality. C1 [Kirschbaum, D. B.; Lerner-Lam, A.] Columbia Univ, Lamont Doherty Geol Observ, Palisades, NY 10964 USA. [Kirschbaum, D. B.; Lerner-Lam, A.] Columbia Univ, Dept Earth & Environm Sci, Palisades, NY USA. [Kirschbaum, D. B.; Adler, R.] NASA, Goddard Space Flight Ctr, Atmospheres Lab, Greenbelt, MD 20771 USA. [Adler, R.] Univ Maryland, ESSIC, College Pk, MD 20742 USA. [Hong, Y.] Univ Oklahoma, Sch Civil Engn & Environm Sci, Natl Weather Ctr, Norman, OK 73019 USA. RP Kirschbaum, DB (reprint author), Columbia Univ, Lamont Doherty Geol Observ, Palisades, NY 10964 USA. EM dbach@ldeo.columbia.edu RI Hong, Yang/D-5132-2009; Kirschbaum, Dalia/F-9596-2012; Namikawa, Laercio/C-5559-2013 OI Hong, Yang/0000-0001-8720-242X; Namikawa, Laercio/0000-0001-7847-1804 FU NASA [NNG05GN31H]; Lamont-Doherty Earth Observatory, Columbia University FX The authors would like to thank Stephanie Hill and Lynne Shupp for their help in preparing the landslide inventory database. This research was supported by a grant from NASA Applied Sciences program, NASA Graduate Fellowship ( Grant NNG05GN31H) and by the Lamont-Doherty Earth Observatory, Columbia University. NR 40 TC 29 Z9 29 U1 2 U2 23 PU COPERNICUS PUBLICATIONS PI KATHLENBURG-LINDAU PA MAX-PLANCK-STR 13, KATHLENBURG-LINDAU, 37191, GERMANY SN 1561-8633 J9 NAT HAZARD EARTH SYS JI Nat. Hazards Earth Syst. Sci. PY 2009 VL 9 IS 3 BP 673 EP 686 PG 14 WC Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences; Water Resources SC Geology; Meteorology & Atmospheric Sciences; Water Resources GA 464XP UT WOS:000267543300003 ER PT J AU Bills, BG AF Bills, Bruce G. TI PLANETARY SCIENCE Tidal flows in satellite oceans SO NATURE GEOSCIENCE LA English DT News Item ID DISSIPATION; EUROPA AB Sub-surface oceans probably exist on several large satellites of Jupiter and Saturn. An analysis of Europa's tides suggests that some of the Rossby waves are resonantly enhanced by the obliquity, producing sufficient heat and flow to keep the ocean liquid. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Bills, BG (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM bruce.bills@jpl.nasa.gov NR 11 TC 5 Z9 5 U1 1 U2 5 PU NATURE PUBLISHING GROUP PI NEW YORK PA 75 VARICK ST, 9TH FLR, NEW YORK, NY 10013-1917 USA SN 1752-0894 J9 NAT GEOSCI JI Nat. Geosci. PD JAN PY 2009 VL 2 IS 1 BP 13 EP 14 DI 10.1038/ngeo396 PG 3 WC Geosciences, Multidisciplinary SC Geology GA 397CB UT WOS:000262638500010 ER PT B AU Hemmati, H AF Hemmati, Hamid BE Hemmati, H TI Near-Earth Laser Communications SO NEAR-EARTH LASER COMMUNICATIONS SE Optical Science and Engineering-CRC LA English DT Article; Book Chapter ID OPTICAL COMMUNICATIONS; SPACE COMMUNICATIONS; PERFORMANCE C1 CALTECH, Jet Prop Lab, NASA, Pasadena, CA 91125 USA. RP Hemmati, H (reprint author), CALTECH, Jet Prop Lab, NASA, Pasadena, CA 91125 USA. NR 61 TC 0 Z9 0 U1 0 U2 0 PU CRC PRESS-TAYLOR & FRANCIS GROUP PI BOCA RATON PA 6000 BROKEN SOUND PARKWAY NW, STE 300, BOCA RATON, FL 33487-2742 USA BN 978-0-8247-5381-8 J9 OPT SCI ENG-CRC PY 2009 BP 1 EP + D2 10.1201/9781420015447 PG 31 WC Engineering, Electrical & Electronic; Optics SC Engineering; Optics GA BJV02 UT WOS:000267226700001 ER PT B AU Pribil, K Hemmati, H AF Pribil, Klaus Hemmati, Hamid BE Hemmati, H TI Laser Transmitters: Coherent and Direct Detections SO NEAR-EARTH LASER COMMUNICATIONS SE Optical Science and Engineering-CRC LA English DT Article; Book Chapter ID PHOTONIC CRYSTAL FIBERS; AMPLIFIERS; POWER C1 [Pribil, Klaus] NewComp, Freienstein, Switzerland. [Hemmati, Hamid] CALTECH, Jet Prop Lab, NASA, Pasadena, CA USA. RP Pribil, K (reprint author), NewComp, Freienstein, Switzerland. NR 20 TC 0 Z9 0 U1 0 U2 1 PU CRC PRESS-TAYLOR & FRANCIS GROUP PI BOCA RATON PA 6000 BROKEN SOUND PARKWAY NW, STE 300, BOCA RATON, FL 33487-2742 USA BN 978-0-8247-5381-8 J9 OPT SCI ENG-CRC PY 2009 BP 97 EP + D2 10.1201/9781420015447 PG 46 WC Engineering, Electrical & Electronic; Optics SC Engineering; Optics GA BJV02 UT WOS:000267226700004 ER PT B AU Hemmati, H AF Hemmati, Hamid BE Hemmati, H TI Flight Optomechanical Assembly SO NEAR-EARTH LASER COMMUNICATIONS SE Optical Science and Engineering-CRC LA English DT Article; Book Chapter C1 CALTECH, Jet Prop Lab, NASA, Pasadena, CA 91125 USA. RP Hemmati, H (reprint author), CALTECH, Jet Prop Lab, NASA, Pasadena, CA 91125 USA. NR 24 TC 0 Z9 0 U1 0 U2 0 PU CRC PRESS-TAYLOR & FRANCIS GROUP PI BOCA RATON PA 6000 BROKEN SOUND PARKWAY NW, STE 300, BOCA RATON, FL 33487-2742 USA BN 978-0-8247-5381-8 J9 OPT SCI ENG-CRC PY 2009 BP 143 EP 160 D2 10.1201/9781420015447 PG 18 WC Engineering, Electrical & Electronic; Optics SC Engineering; Optics GA BJV02 UT WOS:000267226700005 ER PT B AU Moision, B Hamkins, J AF Moision, Bruce Hamkins, Jon BE Hemmati, H TI Coding and Modulation for Free-Space Optical Communications SO NEAR-EARTH LASER COMMUNICATIONS SE Optical Science and Engineering-CRC LA English DT Article; Book Chapter ID CHANNEL; CODES; CAPACITY C1 [Moision, Bruce; Hamkins, Jon] CALTECH, Jet Prop Lab, NASA, Pasadena, CA 91125 USA. RP Moision, B (reprint author), CALTECH, Jet Prop Lab, NASA, Pasadena, CA 91125 USA. NR 29 TC 1 Z9 1 U1 0 U2 0 PU CRC PRESS-TAYLOR & FRANCIS GROUP PI BOCA RATON PA 6000 BROKEN SOUND PARKWAY NW, STE 300, BOCA RATON, FL 33487-2742 USA BN 978-0-8247-5381-8 J9 OPT SCI ENG-CRC PY 2009 BP 161 EP 187 D2 10.1201/9781420015447 PG 27 WC Engineering, Electrical & Electronic; Optics SC Engineering; Optics GA BJV02 UT WOS:000267226700006 ER PT B AU Piazzolla, S AF Piazzolla, Sabino BE Hemmati, H TI Atmospheric Channel SO NEAR-EARTH LASER COMMUNICATIONS SE Optical Science and Engineering-CRC LA English DT Article; Book Chapter ID OPTICAL SCINTILLATIONS; TURBULENT ATMOSPHERE; PROBABILITY-DENSITY; FLUCTUATIONS; PROPAGATION; SYSTEMS; PATH C1 CALTECH, Jet Prop Lab, NASA, Pasadena, CA 91125 USA. RP Piazzolla, S (reprint author), CALTECH, Jet Prop Lab, NASA, Pasadena, CA 91125 USA. NR 34 TC 4 Z9 4 U1 0 U2 0 PU CRC PRESS-TAYLOR & FRANCIS GROUP PI BOCA RATON PA 6000 BROKEN SOUND PARKWAY NW, STE 300, BOCA RATON, FL 33487-2742 USA BN 978-0-8247-5381-8 J9 OPT SCI ENG-CRC PY 2009 BP 237 EP + D2 10.1201/9781420015447 PG 37 WC Engineering, Electrical & Electronic; Optics SC Engineering; Optics GA BJV02 UT WOS:000267226700008 ER PT B AU Hemmati, H AF Hemmati, Hamid BE Hemmati, H TI Reliability and Flight Qualification SO NEAR-EARTH LASER COMMUNICATIONS SE Optical Science and Engineering-CRC LA English DT Article; Book Chapter ID GAMMA-IRRADIATION; LASER-DIODES; DOPED FIBERS; RADIATION; PERFORMANCE; PHOTONICS; PROGRAM C1 CALTECH, Jet Prop Lab, NASA, Pasadena, CA 91125 USA. RP Hemmati, H (reprint author), CALTECH, Jet Prop Lab, NASA, Pasadena, CA 91125 USA. NR 52 TC 0 Z9 0 U1 0 U2 0 PU CRC PRESS-TAYLOR & FRANCIS GROUP PI BOCA RATON PA 6000 BROKEN SOUND PARKWAY NW, STE 300, BOCA RATON, FL 33487-2742 USA BN 978-0-8247-5381-8 J9 OPT SCI ENG-CRC PY 2009 BP 321 EP 343 D2 10.1201/9781420015447 PG 23 WC Engineering, Electrical & Electronic; Optics SC Engineering; Optics GA BJV02 UT WOS:000267226700010 ER PT B AU Hemmati, H AF Hemmati, Hamid BE Hemmati, H TI Future Directions SO NEAR-EARTH LASER COMMUNICATIONS SE Optical Science and Engineering-CRC LA English DT Article; Book Chapter ID OPTICAL COMMUNICATIONS DEMONSTRATOR C1 CALTECH, Jet Prop Lab, NASA, Pasadena, CA 91125 USA. RP Hemmati, H (reprint author), CALTECH, Jet Prop Lab, NASA, Pasadena, CA 91125 USA. NR 17 TC 0 Z9 0 U1 0 U2 0 PU CRC PRESS-TAYLOR & FRANCIS GROUP PI BOCA RATON PA 6000 BROKEN SOUND PARKWAY NW, STE 300, BOCA RATON, FL 33487-2742 USA BN 978-0-8247-5381-8 J9 OPT SCI ENG-CRC PY 2009 BP 369 EP 374 D2 10.1201/9781420015447 PG 6 WC Engineering, Electrical & Electronic; Optics SC Engineering; Optics GA BJV02 UT WOS:000267226700012 ER PT B AU Blackwell, WJ Chen, FW AF Blackwell, William J. Chen, Frederick W. BA Blackwell, WJ Chen, FW BF Blackwell, WJ Chen, FW TI Neural Networks in Atmospheric Remote Sensing Introduction SO NEURAL NETWORKS IN ATMOSPHERIC REMOTE SENSING SE Artech House Remote Sensing Library LA English DT Editorial Material; Book Chapter ID ENVIRONMENTAL SCIENCES C1 [Blackwell, William J.] NASA, AIRS NPP Sci Team, Washington, DC USA. [Chen, Frederick W.] Signal Syst Corp, Severna Pk, MD USA. [Chen, Frederick W.] Argonne Natl Lab, Argonne, IL 60439 USA. [Chen, Frederick W.] MIT, Lincoln Lab, Cambridge, MA 02139 USA. NR 6 TC 19 Z9 19 U1 0 U2 0 PU ARTECH HOUSE PI NORWOOD PA 685 CANTON ST, NORWOOD, MA 02062 USA BN 978-1-59693-372-9 J9 ARTECH HSE REMOTE SE PY 2009 BP 1 EP 5 PG 5 WC Remote Sensing SC Remote Sensing GA BKE03 UT WOS:000267849700001 ER PT S AU Zavlin, VE AF Zavlin, Vyacheslav E. BE Becker, W TI Theory of Radiative Transfer in Neutron Star Atmospheres and Its Applications SO NEUTRON STARS AND PULSARS SE Astrophysics and Space Science Library LA English DT Article; Book Chapter ID MILLISECOND PULSAR J0437-4715; XMM-NEWTON OBSERVATIONS; X-RAY-EMISSION; SUPERNOVA REMNANT IC-443; STRONG MAGNETIC-FIELDS; MODEL ATMOSPHERES; ULTRAVIOLET EMISSION; CHANDRA OBSERVATIONS; THERMAL EMISSION; POLAR CAPS C1 NASA, George C Marshall Space Flight Ctr, Space Sci Lab, Huntsville, AL 35805 USA. RP Zavlin, VE (reprint author), NASA, George C Marshall Space Flight Ctr, Space Sci Lab, SD59, Huntsville, AL 35805 USA. EM vyacheslav.zavlin@msfc.nasa.gov NR 101 TC 23 Z9 23 U1 0 U2 0 PU SPRINGER PI DORDRECHT PA PO BOX 17, 3300 AA DORDRECHT, NETHERLANDS SN 0067-0057 BN 978-3-540-76964-4 J9 ASTROPHYS SPACE SC L PY 2009 VL 357 BP 181 EP 211 D2 10.1007/978-3-540-76965-1 PG 31 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BJO24 UT WOS:000266889500009 ER PT S AU Harding, AK AF Harding, Alice K. BE Becker, W TI High-energy Emission from the Polar Cap and Slot Gap SO NEUTRON STARS AND PULSARS SE Astrophysics and Space Science Library LA English DT Article; Book Chapter ID GAMMA-RAY PULSARS; INVERSE COMPTON-SCATTERING; STRONG MAGNETIC-FIELDS; RADIATION PAIR FRONTS; MILLISECOND PULSARS; PARTICLE-ACCELERATION; RADIO-EMISSION; YOUNG PULSARS; CREATION; MAGNETOSPHERES C1 NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Washington, DC 20546 USA. RP Harding, AK (reprint author), NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Washington, DC 20546 USA. EM harding@twinkie.gsfc.nasa.gov NR 79 TC 9 Z9 9 U1 0 U2 0 PU SPRINGER PI DORDRECHT PA PO BOX 17, 3300 AA DORDRECHT, NETHERLANDS SN 0067-0057 BN 978-3-540-76964-4 J9 ASTROPHYS SPACE SC L PY 2009 VL 357 BP 521 EP 542 D2 10.1007/978-3-540-76965-1 PG 22 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BJO24 UT WOS:000266889500019 ER PT S AU Weisskopf, MC Elsner, RF Kaspi, VM O'Dell, SL George, GP Ramsey, BD AF Weisskopf, Martin C. Elsner, Ronald F. Kaspi, Victoria M. O'Dell, Stephen L. George, G. Pavlov Ramsey, Brain D. BE Becker, W TI X-Ray Polarimetry and Its Potential Use for Understanding Neutron Stars SO NEUTRON STARS AND PULSARS SE Astrophysics and Space Science Library LA English DT Article; Book Chapter ID SOFT GAMMA-REPEATERS; STRONGLY MAGNETIZED PLASMA; RAPIDLY SPINNING PULSARS; COHERENT TIMING SOLUTION; COMPACT CENTRAL OBJECT; CRAB PULSAR; OPTICAL POLARIZATION; OUTER MAGNETOSPHERE; ENERGETIC RADIATION; SCATTERING FACTORS C1 [Weisskopf, Martin C.; Elsner, Ronald F.; O'Dell, Stephen L.; Ramsey, Brain D.] NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA. [Kaspi, Victoria M.] McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada. [George, G. Pavlov] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. RP Weisskopf, MC (reprint author), NASA, George C Marshall Space Flight Ctr, VP62, Huntsville, AL 35812 USA. EM martin@smoker.msfc.nasa.gov; ron.elsner@nasa.gov; vkaspi@hep.physics.mcgill.ca; Steve.O'Dell@nasa.gov; pavlov@astro.psu.edu; Brian.Ramsey@nasa.gov OI O'Dell, Stephen/0000-0002-1868-8056 NR 90 TC 17 Z9 17 U1 0 U2 0 PU SPRINGER PI DORDRECHT PA PO BOX 17, 3300 AA DORDRECHT, NETHERLANDS SN 0067-0057 BN 978-3-540-76964-4 J9 ASTROPHYS SPACE SC L PY 2009 VL 357 BP 589 EP 619 D2 10.1007/978-3-540-76965-1 PG 31 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BJO24 UT WOS:000266889500022 ER PT S AU Smith, DA Thompson, DJ AF Smith, David A. Thompson, David J. BE Becker, W TI GeV Gamma-Ray Pulsar Detection SO NEUTRON STARS AND PULSARS SE Astrophysics and Space Science Library LA English DT Article; Book Chapter ID ATMOSPHERIC CHERENKOV TELESCOPES; HIGH-ENERGY; IMAGING TELESCOPE; CRAB-NEBULA; EMISSION; ARRAY; GLAST; DISCOVERY; ASTRONOMY; VERITAS C1 [Smith, David A.] Univ Bordeaux 1, CENBG UMR 5797, CNRS, IN2P3, F-33175 Gradignan, France. [Thompson, David J.] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20721 USA. RP Smith, DA (reprint author), Univ Bordeaux 1, CENBG UMR 5797, CNRS, IN2P3, 1 Chemin Solarium BP120, F-33175 Gradignan, France. EM smith@cenbg.in2p3.fr; David.J.Thompson@nasa.gov NR 69 TC 1 Z9 1 U1 0 U2 0 PU SPRINGER PI DORDRECHT PA PO BOX 17, 3300 AA DORDRECHT, NETHERLANDS SN 0067-0057 BN 978-3-540-76964-4 J9 ASTROPHYS SPACE SC L PY 2009 VL 357 BP 621 EP 649 D2 10.1007/978-3-540-76965-1 PG 29 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BJO24 UT WOS:000266889500023 ER PT J AU Murphy, PJ AF Murphy, P. J. TI Extended Care SO NEW ENGLAND REVIEW-MIDDLEBURY SERIES LA English DT Fiction, Creative Prose C1 [Murphy, P. J.] Eastfield Coll, Mesquite, TX USA. [Murphy, P. J.] NASA, Washington, DC USA. [Murphy, P. J.] Univ Florida, Masters Program Forens Toxicol, Gainesville, FL 32611 USA. RP Murphy, PJ (reprint author), Univ Florida, Alcohol Testing Program, Gainesville, FL 32611 USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU MIDDLEBURY COLL PUBLICATIONS PI MIDDLEBURY PA MIDDLEBURY COLLEGE, MIDDLEBURY, VT 05753 USA SN 1053-1297 J9 NEW ENGL REV-MIDDLEB JI New Engl. Rev.-Middlebury Ser. PY 2009 VL 30 IS 1 BP 167 EP 179 PG 13 WC Literary Reviews SC Literature GA 435NO UT WOS:000265350800026 ER PT S AU Heap, S Lindler, DJ AF Heap, Sally Lindler, Don J. BE Dagostino, MC Bertone, E Gonzalez, DR TI Constraining Galaxy Evolution With Hubble's Next Generation Spectral Library SO NEW QUESTS IN STELLAR ASTROPHYSICS II: ULTRAVIOLET PROPERTIES OF EVOLVED STELLAR POPULATIONS SE Astrophysics and Space Science Proceedings LA English DT Proceedings Paper CT International Conference on Untraviolet Properties of Evolved Stellar Populations CY APR 16-20, 2007 CL Puerto Vallarta, MEXICO SP Inst Nacl Astrofis, Opt & Elect, Univ Guadalajara ID STARS; MASS AB We present Hubble's Next Generation Spectral Library, a library of UV-optical spectra (0-2 - 1.0 mu) of 378 stars. We show that the mid-UV spectrum can be used to constrain the ages and metallicities of high-redshift galaxies presently being observed with large, ground-based telescopes. C1 [Heap, Sally] NASA, Goddard Space Flight Ctr, Greenbelt, MD USA. [Lindler, Don J.] Sigma Space Corp, Lanham, MD USA. RP Heap, S (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD USA. EM Sally.Heap@nasa.gov; Don.J.Lindler@nasa.gov RI heap, sara/E-2237-2012 NR 8 TC 1 Z9 1 U1 0 U2 0 PU SPRINGER PI NEW YORK PA 233 SPRING STREET, NEW YORK, NY 10013, UNITED STATES SN 1570-6591 BN 978-0-387-87620-7 J9 ASTROPHYSICS SPACE PY 2009 BP 273 EP + DI 10.1007/978-0-387-87621-4_37 PG 2 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BJE77 UT WOS:000265216200037 ER PT B AU Boriah, S Kumar, V Steinbach, M Tan, PN Potter, C Klooster, S AF Boriah, Shyam Kumar, Vipin Steinbach, Michael Tan, Pang-Ning Potter, Christopher Klooster, Steven BE Kargupta, H Han, J Yu, PS Motwani, R Kumar, V TI Detecting Ecosystem Disturbances and Land Cover Change Using Data Mining SO NEXT GENERATION OF DATA MINING SE Chapman & Hall-CRC Data Mining and Knowledge Discovery Series LA English DT Article; Book Chapter ID DEFORESTATION; CLIMATE; SCALE C1 [Boriah, Shyam; Kumar, Vipin; Steinbach, Michael; Tan, Pang-Ning] Univ Minnesota, Dept Comp Sci & Engn, Minneapolis, MN 55455 USA. [Potter, Christopher] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Klooster, Steven] Calif State Univ, Monterey Bay Seaside, CA USA. RP Boriah, S (reprint author), Univ Minnesota, Dept Comp Sci & Engn, Minneapolis, MN 55455 USA. NR 10 TC 1 Z9 1 U1 0 U2 0 PU CHAPMAN & HALL/CRC PRESS PI BOCA RATON PA 6000 BROKEN SOUND PKWY, NW, STE 300, BOCA RATON, FL 33487 USA BN 978-1-4200-8586-0 J9 CH CRC DATA MIN KNOW PY 2009 BP 29 EP 47 PG 19 WC Computer Science, Artificial Intelligence; Computer Science, Information Systems; Computer Science, Theory & Methods SC Computer Science GA BJR30 UT WOS:000267022300002 ER PT J AU Pickett, JS Chen, LJ Santolik, O Grimald, S Lavraud, B Verkhoglyadova, OP Tsurutani, BT Lefebvre, B Fazakerley, A Lakhina, GS Ghosh, SS Grison, B Decreau, PME Gurnett, DA Torbert, R Cornilleau-Wehrlin, N Dandouras, I Lucek, E AF Pickett, J. S. Chen, L. -J. Santolik, O. Grimald, S. Lavraud, B. Verkhoglyadova, O. P. Tsurutani, B. T. Lefebvre, B. Fazakerley, A. Lakhina, G. S. Ghosh, S. S. Grison, B. Decreau, P. M. E. Gurnett, D. A. Torbert, R. Cornilleau-Wehrlin, N. Dandouras, I. Lucek, E. TI Electrostatic solitary waves in current layers: from Cluster observations during a super-substorm to beam experiments at the LAPD SO NONLINEAR PROCESSES IN GEOPHYSICS LA English DT Article CT Nonlinear Wave Workshop 2008 CY APR, 2008 CL Beaulieu, FRANCE ID PROTON CYCLOTRON WAVES; PHASE-SPACE HOLES; ACOUSTIC WAVES; ELECTRIC-FIELD; PLASMA; GENERATION; INSTABILITIES; RECONNECTION; NOISE; POLAR AB Electrostatic Solitary Waves (ESWs) have been observed by several spacecraft in the current layers of Earth's magnetosphere since 1982. ESWs are manifested as isolated pulses (one wave period) in the high time resolution waveform data obtained on these spacecraft. They are thus nonlinear structures generated out of nonlinear instabilities and processes. We report the first observations of ESWs associated with the onset of a super-substorm that occurred on 24 August 2005 while the Cluster spacecraft were located in the magnetotail at around 18-19 R(E) and moving northward from the plasma sheet to the lobes. These ESWs were detected in the waveform data of the WBD plasma wave receiver on three of the Cluster spacecraft. The majority of the ESWs were detected about 5 min after the super-substorm onset during which time 1) the PEACE electron instrument detected significant field-aligned electron fluxes from a few 100 eV to 3.5 keV, 2) the EDI instrument detected bursts of field-aligned electron currents, 3) the FGM instrument detected substantial magnetic fluctuations and the presence of Alfv,n waves, 4) the STAFF experiment detected broadband electric and magnetic waves, ion cyclotron waves and whistler mode waves, and 5) CIS detected nearly comparable densities of H+ and O+ ions and a large tailward H+ velocity. We compare the characteristics of the ESWs observed during this event to those created in the laboratory at the University of California-Los Angeles Plasma Device (LAPD) with an electron beam. We find that the time durations of both space and LAPD ESWs are only slightly larger than the respective local electron plasma periods, indicating that electron, and not ion, dynamics are responsible for generation of the ESWs. We have discussed possible mechanisms for generating the ESWs in space, including the beam and kinetic Buneman type instabilities and the acoustic instabilities. Future studies will examine these mechanisms in more detail using the space measurements as inputs to models, and better relate the ESW space measurements to the laboratory through PIC code models. C1 [Pickett, J. S.; Santolik, O.; Gurnett, D. A.] Univ Iowa, Dept Phys & Astron, Iowa City, IA 52242 USA. [Chen, L. -J.; Lefebvre, B.; Torbert, R.] Univ New Hampshire, Ctr Space Sci, Durham, NH 03824 USA. [Santolik, O.; Grison, B.] Inst Atmospher Phys, Prague, Czech Republic. [Santolik, O.] Charles Univ Prague, Fac Math & Phys, Prague, Czech Republic. [Grimald, S.; Fazakerley, A.] Univ Coll London, Mullard Space Sci Lab, Holmbury, England. [Lavraud, B.; Dandouras, I.] Univ Toulouse UPS, Ctr Etud Spatiale Rayonnements, Toulouse, France. [Lavraud, B.; Dandouras, I.] CNRS, UMR 5187, Toulouse, France. [Verkhoglyadova, O. P.; Tsurutani, B. T.] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Verkhoglyadova, O. P.] Univ Alabama, CSPAR, Huntsville, AL 35899 USA. [Lakhina, G. S.] Indian Inst Geomagnetism, Navi Mumbai, India. [Grison, B.; Cornilleau-Wehrlin, N.] CNRS, LPP, Velizy Villacoublay, France. [Decreau, P. M. E.] CNRS, LPC2E, F-45071 Orleans, France. [Decreau, P. M. E.] Univ Orleans, Orleans, France. [Grison, B.] Estec, ESA, Noordwijk, Netherlands. [Cornilleau-Wehrlin, N.] Observ Paris, Stn Radioastron Nancay, Nancay, France. [Lucek, E.] Univ London Imperial Coll Sci Technol & Med, Blackett Lab, London, England. RP Pickett, JS (reprint author), Univ Iowa, Dept Phys & Astron, Iowa City, IA 52242 USA. EM pickett@uiowa.edu RI Chen, Li-Jen/C-2106-2012; Lakhina, Gurbax /C-9295-2012; Ghosh, Suktisama/J-8494-2013; Santolik, Ondrej/F-7766-2014; Grison, Benjamin/G-9440-2014; OI Grison, Benjamin/0000-0002-3440-6856; Dandouras, Iannis/0000-0002-7121-1118; Lakhina, Gurbax /0000-0002-8956-486X; Verkhoglyadova, Olga/0000-0002-9295-9539 NR 45 TC 11 Z9 11 U1 0 U2 1 PU COPERNICUS PUBLICATIONS PI KATHLENBURG-LINDAU PA MAX-PLANCK-STR 13, KATHLENBURG-LINDAU, 37191, GERMANY SN 1023-5809 J9 NONLINEAR PROC GEOPH JI Nonlinear Process Geophys. PY 2009 VL 16 IS 3 BP 431 EP 442 PG 12 WC Geochemistry & Geophysics; Meteorology & Atmospheric Sciences SC Geochemistry & Geophysics; Meteorology & Atmospheric Sciences GA 464XQ UT WOS:000267543500006 ER PT J AU Cardace, D Hoehler, TM AF Cardace, Dawn Hoehler, Tori M. TI Serpentinizing Fluids Craft Microbial Habitat SO NORTHEASTERN NATURALIST LA English DT Article; Proceedings Paper CT 6th International Conference on Serpentine Ecology CY JUN 16-23, 2008 CL Coll Atlantic, Bar Harbor, ME HO Coll Atlantic ID PARTIAL MOLAL PROPERTIES; HIGH-PRESSURES; TRANSPORT-PROPERTIES; THERMODYNAMIC PROPERTIES; HYDROTHERMAL SYSTEMS; TEMPERATURES; STANDARD; DEEP; SUBSURFACE; BACTERIA AB Hydrogen produced by serpentinization has the potential to fuel subsurface microbial metabolisms. In the serpentinizing subsurface, the solids comprise ultramafic parent rocks derived from the Earth's mantle, serpentine minerals, veins of hydroxides, and accessory magnetite and/or other metal-rich grains. Fluid that occurs with these solids is altered seawater and/or meteoric water and is predicted to be reducing. Hydrogen, a powerful reducing agent, is generated when Fe(2+) in Fe(OH)(2) is oxidized to magnetite, coupled to the reduction of water. Theoretical considerations and experimental work suggest that serpentinization may generate fluid H(2) concentrations as high as approximate to 75 millimolar, and that related seeps on land should have approximate to 300 micromolar. Field observations have shown that submarine serpentinizing seeps contain fluid H(2) concentrations of 1 to 15 millimolar H(2), subseafloor sediments have approximate to 7-100 nanomolar H(2), and thermal springs have approximate to 13 nanomolar H(2). Fluid H(2) has the potential to drive a variety of metabolic processes in oxygen- and organic carbon-deprived environments, such that considerable interest has developed in the potential of serpentinizing systems as an abode of deep subsurface life. Based on empirical parameters, we have modeled the free-energy change for an array of metabolic reactions that may be associated with serpentinization, and find that metabolic niches do exist for methanogenesis, ferric iron reduction, sulfate reduction, and nitrate reduction, given environmentally realistic fluid chemistries. C1 [Cardace, Dawn; Hoehler, Tori M.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Cardace, D (reprint author), NASA, Ames Res Ctr, MS 239-4, Moffett Field, CA 94035 USA. EM dawn.cardace-1@nasa.gov NR 49 TC 12 Z9 13 U1 0 U2 12 PU HUMBOLDT FIELD RESEARCH INST PI STEUBEN PA PO BOX 9, STEUBEN, ME 04680-0009 USA SN 1092-6194 J9 NORTHEAST NAT JI Northeast. Nat PY 2009 VL 16 SI 5 BP 272 EP 284 DI 10.1656/045.016.0520 PG 13 WC Biodiversity Conservation; Ecology SC Biodiversity & Conservation; Environmental Sciences & Ecology GA 585GU UT WOS:000276813900020 ER PT J AU Wargo, AM Tilburg, CE Driggers, WB Sulikowski, JA AF Wargo, Andrew M. Tilburg, Charles E. Driggers, William B. Sulikowski, James A. TI Observations on the Distribution of Ichthyoplankton within the Saco River Estuary System SO NORTHEASTERN NATURALIST LA English DT Article ID LARVAL FISHES; MAINE; ABUNDANCE; DYNAMICS; GULF; BAY AB Determining planktonic larval species composition and abundance data can serve to elucidate local patterns of distribution, determine an area's importance as a nursery ground, and help clarify broad-scale trends of adult distribution and spawning ranges. Although the Saco River and estuary is the fourth largest waterway system in Maine, this ecosystem has remained relatively unstudied over the last thirty years, and research describing the temporal ichthyoplankton composition and distribution is virtually absent. The present study examined the structure of the ichthyoplankton community and determined the temporal and spatial variation in species diversity and abundance within the Saco Bay estuary system. Weekly sampling trips during the months of June, July, and August in 2007 revealed ten species of ichthyoplankton present in the study area. Ulvaria subbifurcata (Radiated Shanny) and Tautogolabrus adsperus (Cunner) dominated the abundance data followed by Hippoglossoides platessoides (American Plaice) and Myoxocephalus octodecims-pinosus (Longhorn Sculpin). C1 [Wargo, Andrew M.; Tilburg, Charles E.; Sulikowski, James A.] Univ New England, Ctr Marine Sci, Biddeford, ME 04005 USA. [Driggers, William B.] SE Fisheries Sci Ctr, Natl Marine Fisheries Serv, Pascagoula, MS 39568 USA. RP Sulikowski, JA (reprint author), Univ New England, Ctr Marine Sci, 11 Hills Beach Rd, Biddeford, ME 04005 USA. EM jsulikowski@une.edu FU University of New England Marine Science Center FX We thank Tim Arienti, Nathan Furey, and Angela Cicia for their help in sample collections. Thanks are further extended to Dr. John Olney for his help in identification of the ichthyoplankton. This project was supported by a University of New England Marine Science Center (MSC) Summer Fellowship to J.A. Sulikowski and C.E. Tilburg. This manuscript represents MSC contribution number 20. NR 10 TC 3 Z9 3 U1 0 U2 4 PU HUMBOLDT FIELD RESEARCH INST PI STEUBEN PA PO BOX 9, STEUBEN, ME 04680-0009 USA SN 1092-6194 J9 NORTHEAST NAT JI Northeast. Nat PY 2009 VL 16 IS 4 BP 647 EP 654 DI 10.1656/045.016.n414 PG 8 WC Biodiversity Conservation; Ecology SC Biodiversity & Conservation; Environmental Sciences & Ecology GA 537IV UT WOS:000273107500014 ER PT B AU Yee, HC Sjogreen, B AF Yee, H. C. Sjoegreen, B. BE Pogorelov, NV Audit, E Colella, P Zank, GP TI On Challenges for Hypersonic Turbulent Simulations SO NUMERICAL MODELING OF SPACE PLASMA FLOWS: ASTRONUM-2008 SE Astronomical Society of the Pacific Conference Series LA English DT Proceedings Paper CT 3rd International Conference on Numerical Modeling of Space Plasma Flows CY JUN 08-13, 2008 CL St Johns, VI SP Univ Calif, Inst Geophys & Planetary Phys, Universe French Commiss Atom Energy, Inst Investigat Fundamental Laws ID FINITE-DIFFERENCE SCHEMES; LARGE-EDDY SIMULATION; SOURCE TERMS; NONOSCILLATORY SCHEMES; NUMERICAL-SOLUTIONS; HYPERBOLIC PROBLEMS; WAVE-PROPAGATION; RESOLUTION; ALGORITHM; EQUATIONS AB This short note discusses some of the challenges for design of suitable spatial numerical schemes for hypersonic turbulent flows, including combustion, and thermal and chemical nonequilibrium flows. Often, hypersonic turbulent flows around re-entry space vehicles and space physics involve mixed steady strong shocks and turbulence with unsteady shocklets. Material mixing in combustion poses additional computational challenges. Proper control of numerical dissipation in numerical methods beyond the standard shock-capturing dissipation at discontinuities is an essential element for accurate and stable simulations of the subject physics. On the one hand, the physics of strong steady shocks and unsteady turbulence/shocklet interactions under the nonequilibrium environment is not well understood. On the other hand, standard and newly developed high order accurate (fourth-order or higher) schemes were developed for homogeneous hyerbolic conservation laws and mixed hyperbolic and parabolic. p partial differential equations (PDEs) (without source terms). The majority of finite rate chemistry and thermal nonequilibrium simulations employ methods for homogeneous time-dependent PDEs with a pointwise evaluation of the source terms. The pointwise evaluation of the source term might not be the best choice for stability, accuracy and minimization of spurious numerics for the overall scheme. C1 [Yee, H. C.] NASA, Ames Res Ctr, Moffett Field, CA 94040 USA. [Sjoegreen, B.] Lawrence Livermore Natl Lab, Livermore, CA 94551 USA. RP Yee, HC (reprint author), NASA, Ames Res Ctr, Moffett Field, CA 94040 USA. EM helen.m.yee@nasa.gov FU NASA Fundamental Aeronautics Hypersonic; U.S. Department of Energy by Lawrence Livermore National Laboratory [DE-AC52-07NA27344] FX The financial support from the NASA Fundamental Aeronautics (Hypersonic) program for the first author is gratefully acknowledged. This work performed under the auspices of the U.S. Department of Energy by Lawrence Livermore National Laboratory under Contract DE-AC52-07NA27344. NR 69 TC 0 Z9 0 U1 0 U2 1 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 978-1-58381-692-9 J9 ASTR SOC P PY 2009 VL 406 BP 61 EP + PG 3 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BJW00 UT WOS:000267287200009 ER PT B AU Usmanov, AV Matthaeus, WH Breech, B Goldstein, ML AF Usmanov, Arcadi V. Matthaeus, William H. Breech, Ben Goldstein, Melvyn L. BE Pogorelov, NV Audit, E Colella, P Zank, GP TI An MHD Solar Wind Model with Turbulence Transport SO NUMERICAL MODELING OF SPACE PLASMA FLOWS: ASTRONUM-2008 SE Astronomical Society of the Pacific Conference Series LA English DT Proceedings Paper CT 3rd International Conference on Numerical Modeling of Space Plasma Flows CY JUN 08-13, 2008 CL St Johns, VI SP Univ Calif, Inst Geophys & Planetary Phys, Universe French Commiss Atom Energy, Inst Investigat Fundamental Laws ID ALFVEN WAVES; FLUCTUATIONS; DISSIPATION; EVOLUTION AB We present initial results from an axisymmetric steady-state solar wind model that describes properties of the large-scale solar wind, interplanetary magnetic field, and turbulence throughout the heliosphere from 0.3 AU to 100 AU. The model is based on numerical solutions of large-scale Reynolds-averaged magnetohydrodynamic (MHD) equations coupled with a set of small-scale transport equations for the turbulence energy, normalized cross-helicity, and correlation scale. The combined set of the time-dependent equations is solved in the frame of reference corotating with the Sun by a time-relaxation method. We use the model to study the global solar wind structure and the distribution of turbulence throughout the heliosphere. C1 [Usmanov, Arcadi V.; Matthaeus, William H.] Univ Delaware, Dept Phys & Astron, Newark, DE 19716 USA. [Usmanov, Arcadi V.; Matthaeus, William H.] Univ Delaware, Bartol Res Inst, Newark, DE 19716 USA. [Usmanov, Arcadi V.; Breech, Ben; Goldstein, Melvyn L.] NASA, Goddard Space Flight Ctr, Code 673, Greenbelt, MD USA. RP Usmanov, AV (reprint author), Univ Delaware, Dept Phys & Astron, Newark, DE 19716 USA. EM arcadi.usmanov@nasa.gov; melvyn.goldstein@gsfc.nasa.gov RI Goldstein, Melvyn/B-1724-2008; Usmanov, Arcadi/A-9860-2013 NR 26 TC 9 Z9 9 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 978-1-58381-692-9 J9 ASTR SOC P PY 2009 VL 406 BP 160 EP + PG 3 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BJW00 UT WOS:000267287200022 ER PT B AU Burlaga, LF AF Burlaga, L. F. BE Pogorelov, NV Audit, E Colella, P Zank, GP TI Tsallis Statistics for Models and Observations of the Heliospheric Magnetic Field SO NUMERICAL MODELING OF SPACE PLASMA FLOWS: ASTRONUM-2008 SE ASTRONOMICAL SOCIETY OF THE PACIFIC CONFERENCE SERIES LA English DT Proceedings Paper CT 3rd International Conference on Numerical Modeling of Space Plasma Flows CY JUN 08-13, 2008 CL St Johns, VI SP Univ Cal, Inst Geophys & Planetary Phys, Universe French Commiss Atom Energy, Inst Investigat Fundamental Laws ID SPEED FLUCTUATIONS; OUTER HELIOSPHERE; BOLTZMANN-GIBBS; 95 AU; EVOLUTION; SCALES AB The solar wind is a driven, open, non-linear, non-equilibrium, complex system. Streams, slow flows, ejecta, shocks, etc. produced near the Sun interact as they move away from the sun to create an evolving complex multiscale structure. During solar maximum, interaction regions merge with increasing distance from the sun, and these merged interaction regions coalesce form Global Merged Interaction Regions (GMIRs) which grow out to approximate to 45 AU and then decay out to 90 AU. One aspect of the statistical structure of the observed fluctuations of the magnetic strength B as a function of distance from the sun and scale can be described by the evolution of the probability distributions of increments of B, which can be described by the q-Gaussian functions of Tsallis statistics. These PDFs can be predicted by a deterministic 1-D multi-fluid MHD model with appropriate boundary conditions. C1 NASA, Goddard Space Flight Ctr, Heliospher Sci Div, Geospace Phys Lab, Greenbelt, MD 20771 USA. RP Burlaga, LF (reprint author), NASA, Goddard Space Flight Ctr, Heliospher Sci Div, Geospace Phys Lab, Code 673,Bldg 21,Rm 244, Greenbelt, MD 20771 USA. EM leonard.f.burlaga@nasa.gov NR 27 TC 0 Z9 0 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 978-1-58381-692-9 J9 ASTR SOC P PY 2009 VL 406 BP 181 EP 188 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BJW00 UT WOS:000267287200024 ER PT B AU Putman, WM Lin, SJ AF Putman, William M. Lin, Shian-Jiann BE Pogorelov, NV Audit, E Colella, P Zank, GP TI A Finite-Volume Dynamical Core on the Cubed-Sphere Grid SO NUMERICAL MODELING OF SPACE PLASMA FLOWS: ASTRONUM-2008 SE Astronomical Society of the Pacific Conference Series LA English DT Proceedings Paper CT 3rd International Conference on Numerical Modeling of Space Plasma Flows CY JUN 08-13, 2008 CL St Johns, VI SP Univ Calif, Inst Geophys & Planetary Phys, Universe French Commiss Atom Energy, Inst Investigat Fundamental Laws ID PARABOLIC METHOD PPM; TRANSPORT; EQUATIONS AB The performance of a multidimensional finite-volume scheme for global atmospheric dynamics is evaluated on the cubed-sphere geometry. The development of the finite-volume dynamical core will be discussed from it's latitude-longitude based origins, to the recent implementation oil the cubed-sphere and future non-hydrostatic formulation. Baroclinic evaluation is performed via a recently developed deterministic initial value baroclinic test case from Jablonowski & Williamson (2006) to assess the evolution of ail idealized baroclinic wave in the Northern Hemisphere for global 3-dimensional atmospheric dynamical cores. Comparisons will be made to the traditional latitude-longitude discretization of the finite-volume dynamical core, as well as a spectral formulation for atmospheric dynamical cores. Finally, a glimpse at the achieved and potential scalability of the cubed-sphere finite-volume dynamical core is discussed. C1 [Putman, William M.] NASA, Goddard Space Flight Ctr, Software Integrat & Visualizat Off, Mail Stop 610-3, Greenbelt, MD 20771 USA. [Lin, Shian-Jiann] NOAA, Geophys Fluid Dynam Lab, Princeton, NJ 08540 USA. RP Putman, WM (reprint author), NASA, Goddard Space Flight Ctr, Software Integrat & Visualizat Off, Mail Stop 610-3, Greenbelt, MD 20771 USA. EM william.m.putman@nasa.gov NR 14 TC 15 Z9 15 U1 0 U2 2 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 978-1-58381-692-9 J9 ASTR SOC P PY 2009 VL 406 BP 268 EP + PG 2 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BJW00 UT WOS:000267287200036 ER PT B AU Smith, SM Zwart, SR Kloeris, V Heer, M AF Smith, Scott M. Zwart, Sara R. Kloeris, Vickie Heer, Martina TI Nutritional Biochemistry of Space Flight SO NUTRITIONAL BIOCHEMISTRY OF SPACE FLIGHT SE Space Science Exploration and Policy LA English DT Editorial Material; Book ID BONE-MINERAL DENSITY; SERUM TRANSFERRIN RECEPTOR; RENAL STONE FORMATION; VITAMIN-D DEFICIENCY; PROLONGED BED REST; BODY IRON STORES; RED-CELL MASS; LONG-DURATION SPACEFLIGHT; URINARY CALCIUM EXCRETION; CORONARY HEART-DISEASE C1 [Smith, Scott M.; Zwart, Sara R.] NASA, Lyndon B Johnson Space Ctr, Nutr Biochem Lab, Human Adaptat & Countermeasures Div,Univ Space Re, Houston, TX 77058 USA. [Kloeris, Vickie] NASA, Lyndon B Johnson Space Ctr, Space Food Syst Lab, Habitabil & Environm Factors Div, Houston, TX 77058 USA. [Heer, Martina] Profil Inst Metab Res, Neuss, Germany. [Heer, Martina] DLR, Inst Aerosp Med, Cologne, Germany. RP Smith, SM (reprint author), NASA, Lyndon B Johnson Space Ctr, Nutr Biochem Lab, Human Adaptat & Countermeasures Div,Univ Space Re, Houston, TX 77058 USA. EM scott.m.smith@nasa.gov; sara.zwart-1@nasa.gov; vickie.l.kloeris@nasa.gov; Martina.Heer@profil-research.de NR 763 TC 22 Z9 23 U1 0 U2 2 PU NOVA SCIENCE PUBLISHERS, INC PI HAUPPAUGE PA 400 OSER AVE, STE 1600, HAUPPAUGE, NY 11788-3635 USA BN 978-1-60741-641-8 J9 SPACE SCI EXPLOR POL PY 2009 BP 1 EP + PG 166 WC Biochemistry & Molecular Biology; Nutrition & Dietetics SC Biochemistry & Molecular Biology; Nutrition & Dietetics GA BLS67 UT WOS:000270952200001 ER PT B AU MacLeod, TC Sims, WH Varnavas, KA Sayyah, R Ho, FD AF MacLeod, Todd C. Sims, W. Herb Varnavas, Kosta A. Sayyah, Rana Ho, Fat D. GP IEEE TI Satellite Test of Radiation Impact on Ramtron 512K FRAM SO NVMTS: 2009 10TH ANNUAL NON-VOLATILE MEMORY TECHNOLOGY SYMPOSIUM LA English DT Proceedings Paper CT 10th Annual Non-Volatile Memory Technology Symposium CY OCT 25-28, 2009 CL Portland, OR DE component; FRAM; Satellite; Radiation Test AB The Memory Test Experiment is a space test of a ferroelectric memory device on a low Earth orbit satellite. The test consists of writing and reading data with a ferroelectric based memory device. Any errors are detected and are stored on board the satellite. The data is send to the ground through telemetry once a day. Analysis of the data can determine the kind of error that was found and will lead to a better understanding of the effects of space radiation on memory systems. The test will be one of the first flight demonstrations of ferroelectric memory in a near polar orbit which allows testing in a varied radiation environment. The memory devices being tested is a Ramtron Inc. 512K memory device. This paper details the goals and purpose of this experiment as well as the development process. The process for analyzing the data to gain the maximum understanding of the performance of the ferroelectric memory device is detailed. C1 [MacLeod, Todd C.; Sims, W. Herb; Varnavas, Kosta A.] NASA, Marshall Space Flight Ctr, Space Syst Dept, Huntsville, AL 35812 USA. [Sayyah, Rana; Ho, Fat D.] Univ Alabama, Dept Elect Engn, Huntsville, AL USA. RP MacLeod, TC (reprint author), NASA, Marshall Space Flight Ctr, Space Syst Dept, Huntsville, AL 35812 USA. EM todd.macleod@nasa.gov NR 4 TC 3 Z9 3 U1 0 U2 0 PU IEEE PI NEW YORK PA 345 E 47TH ST, NEW YORK, NY 10017 USA BN 978-1-4244-4953-8 PY 2009 BP 24 EP + DI 10.1109/NVMT.2009.5429778 PG 2 WC Computer Science, Theory & Methods; Engineering, Electrical & Electronic SC Computer Science; Engineering GA BPF44 UT WOS:000278758600005 ER PT S AU Gross, RS Lavallee, DA Blewitt, G Clarke, PJ AF Gross, Richard S. Lavallee, David A. Blewitt, Geoffrey Clarke, Peter J. BE Sideris, MG TI Consistency of Earth Rotation, Gravity, and Shape Measurements SO OBSERVING OUR CHANGING EARTH SE International Association of Geodesy Symposia LA English DT Proceedings Paper CT General Assembly of the International-Association-of-Geodesy/24th General Assembly of the International-Union-of-Geodesy-and-Geophysics CY JUL 02-13, 2007 CL Perugia, ITALY SP Int Assoc Geodesy, Int Union Geodesy & Geophys DE Earth rotation; Earth shape; Gravity; Surface mass density ID OCEAN TIDES; SEA-LEVEL; MASS AB Degree-2 spherical harmonic coefficients of the surface mass density determined from independent GRACE, SLR, GPS, and Earth rotation measurements are compared to each other and to a model of the surface mass density obtained by summing the contributions of atmospheric pressure, ocean-bottom pressure, land hydrology, and a mass-conserving term. In general, the independent measurements are found to be quite consistent with each other and with the model, with correlations being as high as 0.87 and with the model explaining as much as 88% of the observed variance. But no measurement technique is found to be best overall. For the different degree-2 coefficients, measurements from different techniques are found to agree best with the model. Thus, each measurement technique contributes to understanding the degree-2 surface mass density of the Earth. C1 [Gross, Richard S.] CALTECH, Jet Prop Lab, Mail Stop 238-600,4800 Oak Grove Dr, Pasadena, CA 91109 USA. [Lavallee, David A.; Clarke, Peter J.] Newcastle Univ, Sch Civil Engn & Geosci, Newcastle Upon Tyne NE1 7RU, Tyne & Wear, England. [Blewitt, Geoffrey] Univ Nevada, Nevada Bur, Mines & Geol & Seismol Lab, Reno, NV 89557 USA. RP Gross, RS (reprint author), CALTECH, Jet Prop Lab, Mail Stop 238-600,4800 Oak Grove Dr, Pasadena, CA 91109 USA. RI Clarke, Peter/B-1783-2008; Symposia, IAG/K-2857-2012 OI Clarke, Peter/0000-0003-1276-8300; FU Earth Surface and Interior Focus Area of NASA; NASA [NNG04G099G, NAG5-13683]; UK Natural Environment Research Council [NER/A/S/2001/01166]; Royal Society University Research Fellowship FX We thank the IGS analysis center at Scripps Institution of Oceanography for freely providing GPS SINEX files for use by the geodetic community. The work of one of the authors (RSG) described in this paper was performed at the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. Support for the work of RSG was provided by the Earth Surface and Interior Focus Area of NASA. Support for GB was provided by NASA grants NNG04G099G and NAG5- 13683. PJC acknowledges grant NER/A/S/2001/01166 from the UK Natural Environment Research Council, and DAL was supported by a Royal Society University Research Fellowship. NR 22 TC 3 Z9 3 U1 0 U2 1 PU SPRINGER-VERLAG BERLIN PI BERLIN PA HEIDELBERGER PLATZ 3, D-14197 BERLIN, GERMANY SN 0939-9585 BN 978-3-540-85425-8 J9 IAG SYMP PY 2009 VL 133 BP 463 EP + PG 3 WC Geochemistry & Geophysics; Geology; Geosciences, Multidisciplinary SC Geochemistry & Geophysics; Geology GA BIT95 UT WOS:000262710400056 ER PT S AU Behrend, D Bohm, J Charlot, R Clark, T Corey, B Gipson, J Haas, R Koyama, Y MacMillan, D Malkin, Z Niell, A Nilsson, T Petrachenko, B Rogers, A Tuccari, G Wresnik, J AF Behrend, D. Boehm, J. Charlot, R. Clark, T. Corey, B. Gipson, J. Haas, R. Koyama, Y. MacMillan, D. Malkin, Z. Niell, A. Nilsson, T. Petrachenko, B. Rogers, A. Tuccari, G. Wresnik, J. BE Sideris, MG TI Recent Progress in the VLBI2010 Development SO OBSERVING OUR CHANGING EARTH SE International Association of Geodesy Symposia LA English DT Proceedings Paper CT General Assembly of the International-Association-of-Geodesy/24th General Assembly of the International-Union-of-Geodesy-and-Geophysics CY JUL 02-13, 2007 CL Perugia, ITALY SP Int Assoc Geodesy, Int Union Geodesy & Geophys DE Geodetic VLBI; Next generation VLBI2010; IVS; Monte Carlo simulations ID GEODESY AB From October 2003 to September 2005, the International VLBI Service for Geodesy and Astrometry (IVS) examined current and future requirements for geodetic VLBI, including all components from antennas to analysis. IVS Working Group 3 "VLBI 2010", which was tasked with this effort, concluded with recommendations for a new generation of VLBI systems. These recommendations were based on the goals of achieving I mm measurement accuracy on global baselines, performing continuous measurements for time series of station positions and Earth orientation parameters, and reaching a turnaround time from measurement to initial geodetic results of less than 24 It. To realize these recommendations and goals, along with the need for low cost of construction and operation, requires a complete examination of all aspects of geodetic VLBI including equipment, processes, and observational strategies. Hence, in October 2005, the IVS VLBI2010 Committee (V2C) commenced work on defining the VLBI2010 system specifications. In this paper we give a summary of the recent progress of the VLBI2010 project. C1 [Behrend, D.; Clark, T.; Gipson, J.; MacMillan, D.] NASA, Goddard Space Flight Ctr, NVI Inc, Code 698, Greenbelt, MD 20771 USA. [Boehm, J.] Vienna Univ Technol, Inst Geodesy & Geophys, AT-1040 Vienna, Austria. [Charlot, R.] Observ Bordeaux, CNRS UMR 5804, F-33270 Floirac, France. [Clark, T.; Gipson, J.; MacMillan, D.] NASA, Goddard Space Flight Ctr, NVI Inc, Greenbelt, MD 20771 USA. [Corey, B.; Niell, A.; Rogers, A.] MIT, Haystack Observ, Westford, MA 01886 USA. [Haas, R.; Nilsson, T.] Chalmers, Onala Space Observ, SE-43992 Onsala, Sweden. [Koyama, Y.] Kashima Space Res Ctr, NICT, Kashima, Ibaraki 3148501, Japan. [Malkin, Z.] Pulkovo Observ, St Petersburg 196140, Russia. [Petrachenko, B.] Nat Resources Canada, Geodet Survey Div, Ottawa, ON K1A 0E9, Canada. [Tuccari, G.] INFA, Inst Radioastronomia, IT-96017 Noto, Italy. RP Behrend, D (reprint author), NASA, Goddard Space Flight Ctr, NVI Inc, Code 698, Greenbelt, MD 20771 USA. RI Haas, Rudiger/G-1286-2010; Nilsson, Tobias/D-3764-2012; Symposia, IAG/K-2857-2012; Bohm, Johannes/H-9161-2013; Malkin, Zinovy/C-1560-2008; OI Haas, Rudiger/0000-0003-2681-9228; Nilsson, Tobias/0000-0003-4103-9078; Bohm, Johannes/0000-0002-1208-5473; Malkin, Zinovy/0000-0002-5583-8391; Tuccari, Gino/0000-0001-7175-1977 FU Austrian Science Fund (FWF) [P18404-N10] FX J. Bohm and J. Wresnik are grateful to the Austrian Science Fund (FWF) for supporting this work within Project P18404-N10. NR 14 TC 9 Z9 9 U1 0 U2 4 PU SPRINGER-VERLAG BERLIN PI BERLIN PA HEIDELBERGER PLATZ 3, D-14197 BERLIN, GERMANY SN 0939-9585 BN 978-3-540-85425-8 J9 IAG SYMP PY 2009 VL 133 BP 833 EP + PG 4 WC Geochemistry & Geophysics; Geology; Geosciences, Multidisciplinary SC Geochemistry & Geophysics; Geology GA BIT95 UT WOS:000262710400096 ER PT S AU Fisher, AD VanZwieten, JH VanZwieten, TS AF Fisher, A. D. VanZwieten, J. H., Jr. VanZwieten, T. S. GP IEEE TI Adaptive Control of Small Outboard-Powered Boats for Survey Applications SO OCEANS 2009, VOLS 1-3 SE OCEANS-IEEE LA English DT Proceedings Paper CT Oceans 2009 Conference CY OCT 26-29, 2009 CL Biloxi, MS SP Marine Technol Soc, IEEE Ocean Engn Soc DE Autopilot; Adaptive Control; Neuro-adaptive; Adaptive Augmentation; Adaptive PID; Outboard Motor Control AB Four autopilot controllers have been developed in this work that can both hold a desired heading and follow a straight line. These PID, adaptive PID, neuro-adaptive, and adaptive augmenting control algorithms have all been implemented into a numerical simulation of a 33-foot center console vessel with wind, waves, and current disturbances acting in the perpendicular (across-track) direction of the boat's desired trajectory. Each controller is tested for its ability to follow a desired heading in the presence of these disturbances and then to follow a straight line at two different throttle settings for the same disturbances. These controllers were tuned for an input thrust of 2000 N and all four controllers showed good performance with none of the controllers significantly outperforming the others when holding a constant heading and following a straight line at this engine thrust. Each controller was then tested for a reduced engine thrust of 1200 N per engine where each of the three adaptive controllers reduced heading error and across-track error by approximately 50% after a 300 second tuning period when compared to the fixed gain PID, showing that significant robustness to changes in throttle setting was gained by using an adaptive algorithm. C1 [Fisher, A. D.; VanZwieten, J. H., Jr.] Florida Atlantic Univ, 101 N Beach Rd, Dania, FL 33004 USA. [VanZwieten, T. S.] NASA, Marshall Space Flight Ctr, Huntsville, AL 35812 USA. RP Fisher, AD (reprint author), Florida Atlantic Univ, 101 N Beach Rd, Dania, FL 33004 USA. EM afishe14@fau.edu; jvanzwi@fau.edu; tannen.s.vanzwieten@nasa.gov NR 14 TC 0 Z9 0 U1 0 U2 0 PU IEEE PI NEW YORK PA 345 E 47TH ST, NEW YORK, NY 10017 USA SN 0197-7385 BN 978-1-4244-4960-6 J9 OCEANS-IEEE PY 2009 BP 667 EP + PG 2 WC Engineering, Ocean; Oceanography; Remote Sensing SC Engineering; Oceanography; Remote Sensing GA BPY34 UT WOS:000280322600099 ER PT S AU Small, RJ Campbell, T Teixeira, J Smith, TA Dykes, J Chen, S Allard, R AF Small, R. J. Campbell, T. Teixeira, J. Smith, T. A. Dykes, J. Chen, S. Allard, R. GP IEEE TI Air-Sea Interaction In The Ligurian Sea: Numerical Simulations And In-Situ Data In The Summer Of 2007 SO OCEANS 2009, VOLS 1-3 SE OCEANS-IEEE LA English DT Proceedings Paper CT Oceans 2009 Conference CY OCT 26-29, 2009 CL Biloxi, MS SP Marine Technol Soc, IEEE Ocean Engn Soc ID WESTERN MEDITERRANEAN-SEA; MODEL AB In situ experimental data and numerical model results are presented from the Ligurian Sea in the north-western Mediterranean. Here surface winds are light in summer except during occasional Mistral events which are often associated with cyclogenesis in the lee of the Alps. The Ligurian Sea Air-Sea Interaction Experiment (LASIE07) took place in June 2007, with a focus on the coincident measurement of oceanic and atmospheric boundary layer properties. To help interpret the observational results we use the Coupled Ocean-Atmosphere Mesoscale Prediction System (COAMPS (R)), developed at the Naval Research Laboratory. This system includes an atmospheric sigma coordinate, non-hydrostatic model, coupled to a hydrostatic sigma-z level ocean model (Naval Coastal Ocean Model), using the Earth System Modeling Framework (ESMF). Both models are at high resolution: the inner nest of the COAMPS domain is on a 4 km grid with 40 vertical levels, and that for NCOM on a 2km grid with 50 levels. The coupled model system is evaluated for a month-long simulation which includes data assimilation in the atmosphere but not the ocean. Correlatation coefficients between model and observed values for near-surface wind speeds, and turbulent heat fluxes are above 0.5 (significant at 99%) at a deep water mooring. A comparison of the coupled run with an uncoupled atmospheric run using analysis SST at the surface boundary, both of which use atmospheric data assimilation, does not reveal significant or systematic differences. Therefore a non-assimilating run for the period of a strong wind event (26-29 June), is performed to examine more closely the impact of coupling on the flux fields and SST. Here, the cooling of SST up to 3 degrees C over 72 hours in a fully coupled run affects the surface stress, which is reduced by similar to 20%, and the surface latent heat flux which is reduced by 50%, relative to an uncoupled simulation where the SST is kept fixed at the initial value of the coupled run. In other words, the coupling provides a negative feedback on the surface forcing under strong winds. C1 [Small, R. J.; Campbell, T.; Smith, T. A.; Dykes, J.; Allard, R.] USN, Res Lab, Code 7320,Bldg 1009, Stennis Space Ctr, MS 39529 USA. [Teixeira, J.] NASA, Jet Prop Lab, Pasadena, CA 91109 USA. [Chen, S.] NRL Monterey, Monterey, CA 93943 USA. RP Small, RJ (reprint author), USN, Res Lab, Code 7320,Bldg 1009, Stennis Space Ctr, MS 39529 USA. FU High Performance Computing Modernization Program's Battlespace Environments Institute and NRL's 6.2 Core Program "Battlespace Environment Assessment for Situational Awareness" [PE 0602435N] FX RJS, TC, TAS, and RA were supported by the High Performance Computing Modernization Program's Battlespace Environments Institute and NRL's 6.2 Core Program "Battlespace Environment Assessment for Situational Awareness"(Program Element PE 0602435N). NR 13 TC 0 Z9 0 U1 0 U2 1 PU IEEE PI NEW YORK PA 345 E 47TH ST, NEW YORK, NY 10017 USA SN 0197-7385 BN 978-1-4244-4960-6 J9 OCEANS-IEEE PY 2009 BP 676 EP + PG 3 WC Engineering, Ocean; Oceanography; Remote Sensing SC Engineering; Oceanography; Remote Sensing GA BPY34 UT WOS:000280322600100 ER PT S AU Blonski, S Holekamp, K Spiering, BA AF Blonski, Slawomir Holekamp, Kara Spiering, Bruce A. GP IEEE TI NASA Satellite Monitoring of Water Clarity in Mobile Bay for Nutrient Criteria Development SO OCEANS 2009, VOLS 1-3 SE OCEANS-IEEE LA English DT Proceedings Paper CT Oceans 2009 Conference CY OCT 26-29, 2009 CL Biloxi, MS SP Marine Technol Soc, IEEE Ocean Engn Soc ID ATMOSPHERIC CORRECTION; COASTAL WATERS; ABSORPTION-COEFFICIENTS; CROSS-CALIBRATION; LANDSAT-7 ETM+; TIME-SERIES; MODIS; OCEAN; COLOR; PHYTOPLANKTON AB Water clarity controls the loss of sunlight reaching the underwater habitats. Because many organisms living in estuarine and coastal waters rely on photosynthesis, water clarity needs to be incorporated into protective water quality standards for these valued ecosystems. To develop the protective standards, a better understanding of causes and effects of water clarity variability at local and regional scales is needed. To that end, NASA remote sensing data are being used to monitor water clarity (measured by light attenuation) and the constituents that decrease water clarity (chlorophyll a, total suspended solids, and colored dissolved organic matter) in the estuarine and coastal systems of the northern Gulf of Mexico. The NASA measurements are intended to augment and extend temporal and spatial coverage of water clarity monitoring conducted by the Federal and State environmental agencies in the same areas. The main objective is to develop a methodology for and to demonstrate the feasibility of producing long-term (1984 to present) time series of the water clarity parameters based on combined satellite measurements from the Moderate Resolution Imaging Spectroradiometer (MODIS) instruments deployed on the Aqua and Terra spacecraft and from the Thematic Mapper (TM) and Enhanced Thematic Mapper Plus (ETM+) instruments from the Landsat 4/5 and Landsat 7 spacecraft, respectively. Aqua and Terra MODIS provide daily coverage dating from 2000, while Landsat TM/ETM+ data extend back to 1984, although with frequency of only once per 8 to 16 days. NASA Earth science research results that improved instrument calibration and data processing techniques have enabled merging the time series of observations from Landsat and MODIS. Algorithms for the retrieval of water clarity parameters from satellite data selected for this project are based on the inherent optical properties of water: absorption and scattering of light. The algorithms are refined based on comparison with field data collected during water quality monitoring in Mobile Bay, Alabama. Results of this project will support future interagency collaborative efforts to develop numeric nutrient criteria for estuarine and coastal waters in the Gulf of Mexico and will contribute to addressing the Gulf of Mexico Alliance priority issue of reducing nutrient inputs to coastal ecosystems. C1 [Blonski, Slawomir; Holekamp, Kara] Sci Syst & Applicat Inc, Bldg 1105, Stennis Space Ctr, MS 39529 USA. [Spiering, Bruce A.] NASA, Appl Sci & Technol Project Off, Stennis Space Ctr, MS 39529 USA. RP Blonski, S (reprint author), Sci Syst & Applicat Inc, Bldg 1105, Stennis Space Ctr, MS 39529 USA. FU Science Systems and Applications, Inc; NASA at the John C. Stennis Space Center; Mississippi [NNS04AB54T] FX Participation in this research by Science Systems and Applications, Inc., was supported by NASA at the John C. Stennis Space Center, Mississippi, under Task Order NNS04AB54T. NR 19 TC 0 Z9 0 U1 1 U2 5 PU IEEE PI NEW YORK PA 345 E 47TH ST, NEW YORK, NY 10017 USA SN 0197-7385 BN 978-1-4244-4960-6 J9 OCEANS-IEEE PY 2009 BP 1117 EP + PG 2 WC Engineering, Ocean; Oceanography; Remote Sensing SC Engineering; Oceanography; Remote Sensing GA BPY34 UT WOS:000280322600165 ER PT S AU Kalcic, M Hall, C Russell, J Fletcher, R AF Kalcic, Maria Hall, Callie Russell, Jeff Fletcher, Rose GP IEEE TI Monitoring Coastal Marshes for Persistent Saltwater Intrusion SO OCEANS 2009, VOLS 1-3 SE OCEANS-IEEE LA English DT Proceedings Paper CT Oceans 2009 Conference CY OCT 26-29, 2009 CL Biloxi, MS SP Marine Technol Soc, IEEE Ocean Engn Soc AB Saltwater flooding of coastal marshes by storm surge, rising sea level, and subsidence is a primary cause of wetland deterioration and habitat loss. The objective of this study is to provide resource managers with remote sensing products that support ecosystem-forecasting models requiring inundation data. This investigation employed time-series indices derived from 250-meter NASA Moderate Resolution Imaging Spectroradiometer (MODIS) and 30-m Landsat imagery to map flooding and saltwater stress in the Sabine Basin in southwest Louisiana, before and after Hurricane Rita in 2005. After nearly 20 feet of storm surge inundated the area during Hurricane Rita, Hurricane Ike produced a storm surge of almost 14 feet in the same area and flooded areas as far as 30 miles inland. The study design of this investigation centered upon the use of vegetation and wetness (water) indicators to map flooded areas. The study team assigned a vegetation index to marsh areas of concomitant vegetation and water. We derived daily MODIS time series of Normalized Difference Vegetation Index, Normalized Difference Water Index, and Normalized Difference Soil Index from the NASA Stennis Space Center Time Series Product Tool, which provides the capability to compute phenological parameters and performs temporal modeling at ecosystem scales. We estimated the extent of flooding as the percentage of time the MODIS index was water; i.e., below a certain threshold. The percentages indicate areas of persistent flooding over certain time intervals, thereby informing planners of areas with a high probability of conversion to open water. The study team used Landsat 5 and 7 data for the years 2004 through 2006 to produce an 8-day time series of vegetation and wetness indices. We evaluated these Landsat-based flood maps with lidar data and in situ elevation data collected by the U.S. Geological Survey (USGS) and Louisiana Department of Natural Resources Coastwide Reference Monitoring System for the Sabine Basin. Finally, we combined salinity data collected in situ from the USGS and from the National Oceanic and Atmospheric Administration with our flooding estimates to map areas of persistent saltwater intrusion. The combination of these data are useful for habitat switching modules that predict the migration of marsh species from one salinity regime to another from estimates of the annual percent inundation and the mean annual salinity. C1 [Kalcic, Maria; Fletcher, Rose] Sci Syst & Applicat Inc, Bldg 1105, John C Stennis Space Ctr, MS 39529 USA. [Hall, Callie] NASA, Stennis Space Ctr, MS 39529 USA. [Russell, Jeff] CSC, Stennis Space Ctr, MS 39529 USA. RP Kalcic, M (reprint author), Sci Syst & Applicat Inc, Bldg 1105, John C Stennis Space Ctr, MS 39529 USA. FU Science Systems and Applications, Inc; NASA at the John C. Stennis Space Center, Mississippi [NNS04AB54T] FX The authors wish to thank Mr. Abe Dailey, who worked at NASA/SSC as a summer student from the University of Southern Maine. He was responsible for compiling the many sources of data and for producing the salinity data grids. Participation in this work by Science Systems and Applications, Inc. was supported by NASA under Task Order NNS04AB54T at the John C. Stennis Space Center, Mississippi. NR 6 TC 0 Z9 0 U1 2 U2 5 PU IEEE PI NEW YORK PA 345 E 47TH ST, NEW YORK, NY 10017 USA SN 0197-7385 BN 978-1-4244-4960-6 J9 OCEANS-IEEE PY 2009 BP 1150 EP + PG 2 WC Engineering, Ocean; Oceanography; Remote Sensing SC Engineering; Oceanography; Remote Sensing GA BPY34 UT WOS:000280322600169 ER PT S AU Spruce, J Ellis, J Smoot, J Swann, R Graham, W AF Spruce, Joseph Ellis, Jean Smoot, James Swann, Roberta Graham, William GP IEEE TI A Landsat-based Assessment of Mobile Bay Land Use and Land Cover Change from 1974 to 2008 SO OCEANS 2009, VOLS 1-3 SE OCEANS-IEEE LA English DT Proceedings Paper CT Oceans 2009 Conference CY OCT 26-29, 2009 CL Biloxi, MS SP Marine Technol Soc, IEEE Ocean Engn Soc ID COASTAL; LOUISIANA AB This paper discusses results of a Gulf of Mexico Application Pilot project conducted in 2008 to quantify and assess land use land cover (LULC) change from 1974 to 2008. Led by NASA Stennis Space Center, this project involved multiple Gulf of Mexico Alliance (GOMA) partners, including the Mobile Bay National Estuary Program (NEP), the U.S. Army Corps of Engineers, the National Oceanic and Atmospheric Administration's (NOAA's) National Coastal Data Development Center (NCDDC), and the NOAA Coastal Services Center. The Mobile Bay region provides great economic and ecologic benefits to the Nation, including important coastal habitat for a broad diversity of fisheries and wildlife. The Mobile Bay region has experienced considerable LULC change since the latter half of the 20th century. Accompanying this change has been urban expansion and a reduction of rural land uses. Much of this LULC change (largely urbanization) has reportedly occurred since the landfall of Hurricane Frederic in 1979. Regional urbanization threatens the estuary's water quality and aquatic-habitat dependent biota, including commercial fisheries and avian wildlife. Coastal conservation and urban land use planners require additional information on historical LULC change to support coastal habitat restoration and resiliency management efforts. This project quantified and assessed LULC change across the 34-year time frame and at decadal and mid-decadal scales. Nine Landsat images were employed to compute LULC products because of their availability and suitability for the application. The project also used Landsat-based national LULC products, including coastal LULC products from NOAA's Coastal Change & Analysis Program (C-CAP), available at 5-year intervals since 1995. Our study was initiated in part because C-CAP LULC products were not available to assess the region's urbanization prior to 1995 and subsequent to post-Hurricane Katrina in 2006. The study area included the majority of Mobile and Baldwin counties that encompass Mobile Bay. Each date of Landsat data was classified using an end-user defined modified Anderson level 1 classification scheme. LULC classifications were refined using a decision rule approach in conjunction with available C-CAP products. Individual dates of LULC classifications were validated by image interpretation of stratified random locations on raw Landsat color composite imagery in combination with higher resolution remote sensing and in situ reference data. Overall classification accuracies for five separate single-date products ranged from 83% to 89%. The results of the LULC change analysis indicate that during the 34-year study period, urban areas increased from 96,688 to 150,227 acres, representing a 55.37% increase, or 1.63% per annum. Most of the identified urban expansion regarded the conversion of rural forest and agriculture to urban cover types. Final LULC mapping and metadata products were produced for the entire study area as well as for multiple watersheds of concern within the study area. The final project products, including LULC trend information, were incorporated into the Mobile Bay NEP State of the Bay report. Products and metadata were also transferred to NOAA NCDDC to allow free online accessibility and use by COMA partners and by the public. C1 [Spruce, Joseph; Smoot, James] Sci Syst & Applicat Inc, Stennis Space Ctr, MS 39525 USA. [Ellis, Jean] Univ South Carolina, Columbia, SC 29208 USA. [Swann, Roberta] Mobile Bay Natl Estuary Program, Mobile, AL 36615 USA. [Graham, William] NASA, Stennis Space Ctr, MS 39529 USA. RP Spruce, J (reprint author), Sci Syst & Applicat Inc, Stennis Space Ctr, MS 39525 USA. FU NASA's Applied Science and Technology Project Office FX NASAs Applied Science and Technology Project Office supported J. Ellis. T. McPherson assisted with project management. NR 19 TC 0 Z9 0 U1 0 U2 4 PU IEEE PI NEW YORK PA 345 E 47TH ST, NEW YORK, NY 10017 USA SN 0197-7385 BN 978-1-4244-4960-6 J9 OCEANS-IEEE PY 2009 BP 1185 EP + PG 2 WC Engineering, Ocean; Oceanography; Remote Sensing SC Engineering; Oceanography; Remote Sensing GA BPY34 UT WOS:000280322600175 ER PT S AU Spruce, JP Smoot, J Graham, W AF Spruce, J. P. Smoot, J. Graham, W. GP IEEE TI Developing New Coastal Forest Restoration Products Based on Landsat, ASTER, and MODIS Data SO OCEANS 2009, VOLS 1-3 SE OCEANS-IEEE LA English DT Proceedings Paper CT Oceans 2009 Conference CY OCT 26-29, 2009 CL Biloxi, MS SP Marine Technol Soc, IEEE Ocean Engn Soc ID EASTERN-UNITED-STATES; NOAA AVHRR; IMAGERY; TM; WETLANDS; IMPACT; DAMAGE; COVER AB This paper discusses an ongoing effort to develop new geospatial information products for aiding coastal forest restoration and conservation efforts in coastal Louisiana and Mississippi. This project employs Landsat, Advanced Spaceborne Thermal Emission and Reflection Radiometer (ASTER), and Moderate Resolution Imaging Spectroradiometer (MODIS) satellite data in conjunction with airborne elevation data to compute coastal forest cover type maps and change detection products. Improved forest mapping products are needed to aid coastal forest restoration and management efforts of State and Federal agencies in the Northern Gulf of Mexico (NGOM) region. In particular, such products may aid coastal forest land acquisition and conservation easement procurements. This region's forests are often disturbed and subjected to multiple biotic and abiotic threats, including subsidence, salt water intrusion, hurricanes, sea-level rise, insect-induced defoliation and mortality, altered hydrology, wildfire, and conversion to non-forest land use. In some cases, such forest disturbance has led to forest loss or loss of regeneration capacity. In response, a case study was conducted to assess and demonstrate the potential of satellite remote sensing products for improving forest type maps and for assessing forest change over the last 25 years. Change detection products are needed for assessing risks for specific priority coastal forest types, such as live oak and baldcypress-dominated forest. Preliminary results indicate Landsat time series data are capable of generating the needed forest type and change detection products. Useful classifications were obtained using 2 strategies: 1) general forest classification based on use of 3 seasons of Landsat data from the same year; and 2) classification of specific forest types of concern using a single date of Landsat data in which a given targeted type is spectrally distinct compared to adjacent forested cover. When available, ASTER data was useful as a complement to Landsat data. Elevation data helped to define areas in which targeted forest types occur, such as live oak forests on natural levees. MODIS Normalized Difference Vegetation Index time series data aided visual assessments of coastal forest damage and recovery from hurricanes. Landsat change detection products enabled change to be identified at the stand level and at 10-year intervals with the earliest date preceding available change detection products from the National Oceanic and Atmospheric Administration and from the U.S. Geological Survey. Additional work is being done in collaboration with State and Federal agency partners in a follow-on NASA ROSES project to refine and validate these new, promising products. The products from the ROSES project will be available for aiding NGOM coastal forest restoration and conservation. C1 [Spruce, J. P.; Smoot, J.] Sci Syst & Applicat Inc, Bldg 1105, Stennis Space Ctr, MS 39529 USA. [Graham, W.] NASA, Appl Sci & Technol Project Off, Stennis Space Ctr, MS 39529 USA. RP Spruce, JP (reprint author), Sci Syst & Applicat Inc, Bldg 1105, Stennis Space Ctr, MS 39529 USA. FU NASA [NNS04AB54T] FX Participation in this research by Science Systems and Applications, Inc., was supported by NASA at the John C. Stennis Space Center, Mississippi, under Task Order NNS04AB54T. NR 27 TC 0 Z9 0 U1 0 U2 1 PU IEEE PI NEW YORK PA 345 E 47TH ST, NEW YORK, NY 10017 USA SN 0197-7385 BN 978-1-4244-4960-6 J9 OCEANS-IEEE PY 2009 BP 1265 EP + PG 3 WC Engineering, Ocean; Oceanography; Remote Sensing SC Engineering; Oceanography; Remote Sensing GA BPY34 UT WOS:000280322600187 ER PT S AU Alsweiss, S Laupattarakasem, P El-Nimri, S Jones, WL Veleva, S Stiles, BW Rodriguez, E Gaston, RW AF Alsweiss, Suleiman Laupattarakasem, Peth El-Nimri, Salem Jones, W. Linwood Veleva, Svetla Stiles, Bryan W. Rodriguez, Ernesto Gaston, Robert W. GP IEEE TI Simulated OVW Retrievals in Tropical Cyclones for the Next Generation Dual Frequency Scatterometer SO OCEANS 2009, VOLS 1-3 SE OCEANS-IEEE LA English DT Proceedings Paper CT Oceans 2009 Conference CY OCT 26-29, 2009 CL Biloxi, MS SP Marine Technol Soc, IEEE Ocean Engn Soc AB The purpose of this study is to investigate the potential of the next generation Dual Frequency Scatterometer (DFS) proposed to fly onboard the Japanese Aerospace Exploration Agency (JAXA)/GCOM-W2 future mission to measure surface ocean vector winds. An end-to-end simulation was performed to retrieve ocean vector winds in extreme weather conditions, where high winds are usually associated with high rain rates. Both C- and Ku-bands DFS active measurements were combined in the retrieval algorithm. The simultaneous observations of JAXA's Advanced Microwave Scanning Radiometer (AMSR) were used to passively model both the atmospheric attenuation and rain volume backscatter to correct for rain effects and to further improve the retrievals range for tropical cyclones beyond that exhibited by the current operating scatterometers. C1 [Alsweiss, Suleiman; Laupattarakasem, Peth; El-Nimri, Salem; Jones, W. Linwood] Univ Cent Florida, Cent Florida Remote Sensing Lab, Orlando, FL 32816 USA. [Veleva, Svetla; Stiles, Bryan W.; Rodriguez, Ernesto; Gaston, Robert W.] Jet Propuls Lab, Pasadena, CA USA. RP Alsweiss, S (reprint author), Univ Cent Florida, Cent Florida Remote Sensing Lab, Orlando, FL 32816 USA. EM suleimanalsweiss@gmail.com FU DFS Project of the Jet Propulsion Laboratory FX This work was sponsored by the DFS Project of the Jet Propulsion Laboratory, Pasadena, CA. NR 8 TC 0 Z9 0 U1 0 U2 0 PU IEEE PI NEW YORK PA 345 E 47TH ST, NEW YORK, NY 10017 USA SN 0197-7385 BN 978-1-4244-4960-6 J9 OCEANS-IEEE PY 2009 BP 1903 EP + PG 2 WC Engineering, Ocean; Oceanography; Remote Sensing SC Engineering; Oceanography; Remote Sensing GA BPY34 UT WOS:000280322601001 ER PT S AU Ladner, S Arnone, R Sandidge, J Ko, DS Casey, B Hall, C AF Ladner, Sherwin Arnone, Robert Sandidge, Juanita Ko, DongShan Casey, Brandon Hall, Callie GP IEEE TI "Ocean Weather" in the Gulf of Mexico: Exploiting Real-Time Satellite Ecological Properties and Circulation Models for Coastal Ocean Monitoring SO OCEANS 2009, VOLS 1-3 SE OCEANS-IEEE LA English DT Proceedings Paper CT Oceans 2009 Conference CY OCT 26-29, 2009 CL Biloxi, MS SP Marine Technol Soc, IEEE Ocean Engn Soc ID COLOR AB The fusion of real-time remote sensing imagery with numerical ocean circulation models provides a unique capability for monitoring the coastal ocean. A real-time ocean monitoring system is currently operating in the Gulf of Mexico. Dynamic changes in the ocean environment occur on scales of hours, days, weeks and years, which influence biological, ecological and physical processes. By monitoring these processes at different spatial resolutions, new enhanced capability is available to coastal managers and researchers for making decisions. Monitoring of physical processes and bio-optical responses are currently being done for the Gulf of Mexico. Open ocean eddies and loop current interact with coastal processes such as river plumes and tides and have significant impact on the biological and ecological processes along our shores. Until now we had no capability to routinely monitor these ocean conditions without insitu sensors and observations. Now the "weather" in the Gulf of Mexico is being monitored daily and provides coastal managers and researchers an edge in tracking or pin-pointing events. This information assists the decision maker in identifying how physical events are influencing the coastal ecosystem. How is this being done? Improved bio-optical algorithms have been developed and applied to ocean color satellite imagery from NASA's Moderate Resolution Imaging Spectroradiometer (MOD'S) providing estimates of water constituents such as absorption properties from phytoplankton, color dissolved organic matter (CDOM), and detritus and backscattering properties related to sediment concentration. In addition, advances in numerical circulation modeling (Navy Coastal Ocean Model - NCOM) provide nowcasts and forecasts of coastal processes (currents, sea surface height, salinity and temperature). Physical ocean properties of temperature, salinity, and currents from NCOM are combined with daily latest pixel composite products of phytoplankton, CDOM, and detritus absorption, backscattering and sea surface temperature (SST). We demonstrate an advanced environmental monitoring capability available operationally that highlights the fusion of physical (model) and bio-optical properties (satellite). The entire Gulf conditions are demonstrated daily in addition to higher resolution monitoring of coastal conditions. We will focus on Mississippi and Louisiana Coast using high resolution (250 meter resolution) MODIS imagery. We will demonstrate a capability of supporting coastal manager's and researchers integrating satellite bio-optical products, model circulation (current vectors), sea surface height (contours), salinity (contours) and temperature (contours) layers into Google Earth. In addition, we will demonstrate promising new research using satellite optics and numerical models to create surface optical forecast (hourly increments up to 48 hours) and a 3-D optical volume of the ocean derived from a physical (model) / optical (satellite) Gaussian relationship optimized using insitu profiles. By using these methods of fusing the satellite and ocean circulation model it will provide coastal zone managers with a new capability to assess, predict and track Harmful Algal Blooms, Hypoxia, and sediment discharge. C1 [Ladner, Sherwin; Casey, Brandon] QinetiQ North Amer, Bldg 1009,Room 127A, Stennis Space Ctr, MS 39529 USA. [Arnone, Robert; Sandidge, Juanita; Ko, DongShan] US Navy, Res Lab, Stennis Space Ctr, MS 39529 USA. [Hall, Callie] NASA, Stennis Space Ctr, MS 39529 USA. RP Ladner, S (reprint author), QinetiQ North Amer, Bldg 1009,Room 127A, Stennis Space Ctr, MS 39529 USA. FU NOAA NCDDC; NOAA NOS; NOAA NESDIS; NASA Research; Applications Solution Network (REASoN) [CAN-020ES-01] FX The authors would like to thank NOAA NCDDC, NOAA NOS, and NOAA NESDIS for all of their support during this project. Funding for this project was provided by the NASA Research, Education, and Applications Solution Network (REASoN) CAN-020ES-01. NR 10 TC 0 Z9 0 U1 0 U2 0 PU IEEE PI NEW YORK PA 345 E 47TH ST, NEW YORK, NY 10017 USA SN 0197-7385 BN 978-1-4244-4960-6 J9 OCEANS-IEEE PY 2009 BP 2540 EP + PG 2 WC Engineering, Ocean; Oceanography; Remote Sensing SC Engineering; Oceanography; Remote Sensing GA BPY34 UT WOS:000280322601101 ER PT S AU Dennis, SM AF Dennis, Steven M. GP IEEE TI Coverage Metric for Acoustic Receiver Evaluation and Track Generation SO OCEANS 2009, VOLS 1-3 SE OCEANS-IEEE LA English DT Proceedings Paper CT Oceans 2009 Conference CY OCT 26-29, 2009 CL Biloxi, MS SP Marine Technol Soc, IEEE Ocean Engn Soc AB Acoustic receiver track generation has been the subject of active research, both academic and operational, since at least 1946. In general, track generation algorithms operate by maximizing some measure of effectiveness or performance for a particular receiver in a particular environment. Current probability-based receiver performance measures are difficult to visualize, time consuming to calculate and are not easily subject to strict scientific analysis. Although great strides have been made in the ability to model and predict oceanography (temperature, salinity, currents, etc.) accurately, there exists the need to develop measures of receiver performance which more readily lend themselves to analysis of sensitivity to environmental variation or uncertainty. With the increasing dependence on optimization algorithms in acoustic receiver placement and track generation in the presence of variable or uncertain environments, the desire for a more environmentally-sensitive metric of acoustic receiver performance has arisen. A measure of performance based upon acoustic coverage area has shown promise as a basis for acoustic receiver utilization and optimized track generation applications and is presented here. Coverage can be defined as the areas throughout which a receiver has a sufficiently high signal-to-noise ratio or, alternatively, probability of making positive observations. For the purposes of determining optimal receiver placement and track generation the area of interest is divided into a sufficiently sampled grid of calculation points. Computing and compiling acoustic receiver coverage area information for grid points throughout the area of interest into an acoustic receiver coverage map gives immediate visual feedback on locations of optimal performance for a specific acoustic receiver in use in the current ocean environment. By making use of multiple calculation layers in an N x 2-D fashion, acoustic coverage volumes can be constructed for the purposes of three dimensional receiver placement or track generation. The use of an acoustic coverage-based metric for optimal track generation is shown to compare favorably with current track optimizers which use cumulative probability measures of performance, offering faster calculation times and a stronger connection to the acoustic environment. C1 USN, Res Lab, Stennis Space Ctr, Stennis Space Ctr, MS 39529 USA. RP Dennis, SM (reprint author), USN, Res Lab, Stennis Space Ctr, Stennis Space Ctr, MS 39529 USA. NR 10 TC 0 Z9 0 U1 0 U2 0 PU IEEE PI NEW YORK PA 345 E 47TH ST, NEW YORK, NY 10017 USA SN 0197-7385 BN 978-1-4244-4960-6 J9 OCEANS-IEEE PY 2009 BP 2716 EP 2719 PG 4 WC Engineering, Ocean; Oceanography; Remote Sensing SC Engineering; Oceanography; Remote Sensing GA BPY34 UT WOS:000280322601126 ER PT B AU Jones, JA Chao, Y AF Jones, Jack A. Chao, Yi GP ASME TI OFFSHORE HYDROKINETIC ENERGY CONVERSION FOR ONSHORE POWER GENERATION SO OMAE 2009, VOL 4, PTS A AND B LA English DT Proceedings Paper CT 28th International Conference on Ocean, Offshore and Arctic Engineering CY MAY 31-JUN 05, 2009 CL Honolulu, HI SP ASME, Ocean, Offshore & Arctic Engn Div AB Design comparisons have been performed for a number of different tidal energy systems, including a fully submerged, horizontal-axis electro-turbine system, similar to Verdant Tidal Turbines in New York's East River, a platform-based Marine Current Turbine, now operating in Northern Ireland's Strangford Narrows, and the Rotech Lunar Energy system, to be installed off the South Korean Coast. A fourth type of tidal energy system studied is a novel JPL/Caltech hydraulic energy transfer system that uses submerged turbine blades which are mechanically attached to adjacent high-pressure pumps, instead of to adjacent electrical turbines. The generated high-pressure water streams are combined and transferred to an onshore hydroelectric plant by means of a closed-cycle pipeline. The hydraulic energy transfer system was found to be cost competitive, and it allows all electronics to be placed onshore, thus greatly reducing maintenance costs and corrosion problems. It also eliminates the expenses of conditioning and transferring multiple offshore power lines and of building offshore platforms embedded in the sea floor. For time-dependent tidal energy, the pressurized hydraulic energy can be stored in an elevated onshore reservoir that can be used as per consumer energy demand, rather than as per tidal energy supply. This technology is a spinoff of a miniature ocean hydraulic energy transfer system that JPL is developing for the Office of Naval Research (ONR). The ONR device uses ocean temperature differences to provide pressurized hydraulic energy which supplies all electrical power for small submersibles. This type of hydraulic energy device is expected to allow submersibles to stay submerged for years. A three-month ocean endurance test is scheduled for late 2009. Similar types of hydraulic energy transfer systems are potentially applicable to all types of hydrokinetic energy, including free-flowing rivers, ocean wave energy, and energy from ocean currents, such as the Gulf Stream. In each case, the corrosion-prone, submerged electrical turbines are replaced by all-mechanical water pumps without any electrical components, and the energy is hydraulically transferred to remote onshore hydroelectric plants by inexpensive pipes. The submerged mechanical turbine blade/pump assemblies can be attached by long, small-diameter, flexible pressurized lines to the larger submerged, stationary pipe lines, thus allowing the submerged blade/pump assemblies to be lifted to the surface and serviced by boat. Check valves in the flexible lines allow damaged turbine blade/pump assemblies to be automatically taken off-line and later repaired or replaced as required. C1 [Jones, Jack A.] CALTECH, Jet Prop Lab, Mech Syst Div, Pasadena, CA 91125 USA. RP Jones, JA (reprint author), CALTECH, Jet Prop Lab, Mech Syst Div, Pasadena, CA 91125 USA. NR 16 TC 0 Z9 0 U1 0 U2 11 PU AMER SOC MECHANICAL ENGINEERS PI NEW YORK PA THREE PARK AVENUE, NEW YORK, NY 10016-5990 USA BN 978-0-7918-4344-4 PY 2009 BP 993 EP 1002 PG 10 WC Engineering, Ocean; Engineering, Mechanical SC Engineering GA BTB79 UT WOS:000286404300114 ER PT B AU VanZwieten, TS VanZwieten, JH Balas, MJ Driscoll, FR AF VanZwieten, Tannen S. VanZwieten, James H. Balas, Mark J. Driscoll, Frederick R. GP ASME TI DIRECT ADAPTIVE REJECTION OF VORTEX-INDUCED DISTURBANCES FOR A POWERED SPAR PLATFORM SO OMAE 2009, VOL 5 LA English DT Proceedings Paper CT 28th International Conference on Ocean, Offshore and Arctic Engineering CY MAY 31-JUN 05, 2009 CL Honolulu, HI SP ASME, Ocean, Offshore & Arctic Engn Div ID INDUCED VIBRATIONS AB The Rapidly Deployable Stable Platform (RDSP) is a novel vessel designed to be a reconfigurable, stable at-sea platform. It consists of a detachable catamaran and spar, performing missions with the spar extending vertically below the catamaran and hoisting it completely out of the water. Multiple thrusters located along the spar allow it to be actively controlled in this configuration. A controller is presented in this work that uses an adaptive feedback algorithm in conjunction with Direct Adaptive Disturbance Rejection (DADR) to mitigate persistent, vortex-induced disturbances. Given the frequency of a disturbance, the nominal DADR scheme adaptively compensates for its unknown amplitude and phase. This algorithm is extended to adapt to a disturbance frequency that is only coarsely known by including a Phase Locked Loop (PLL). The PLL improves the frequency estimate on-line, allowing the modified controller to reduce vortex-induced motions by more than 95% using achievable thrust in-puts. C1 [VanZwieten, Tannen S.] NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA. RP VanZwieten, JH (reprint author), Florida Atlantic Univ, Dept Ocean Engn, Dania, FL 33004 USA. EM tannen.s.vanzwieten@nasa.gov; jvanzwi@fau.edu; mbalas@uwyo.edu; rdriscol@fau.edu NR 36 TC 0 Z9 0 U1 1 U2 1 PU AMER SOC MECHANICAL ENGINEERS PI NEW YORK PA THREE PARK AVENUE, NEW YORK, NY 10016-5990 USA BN 978-0-7918-4345-1 PY 2009 BP 487 EP 497 PG 11 WC Engineering, Marine; Engineering, Ocean SC Engineering GA BRL02 UT WOS:000282991700053 ER PT S AU Ansari, RR Jones, JA Pollonini, L Rodriguez, M Opperman, R Hochstein, J AF Ansari, Rafat R. Jones, Jeffrey A. Pollonini, Luca Rodriguez, Mikael Opperman, Roedolph Hochstein, Jason BE Cote, GL TI A Non-Invasive Miniaturized-Wireless Laser-Doppler Fiber-Optic Sensor for Understanding Distal Fingertip Injuries in Astronauts SO OPTICAL DIAGNOSTICS AND SENSING IX SE Proceedings of SPIE-The International Society for Optical Engineering LA English DT Proceedings Paper CT Conference on Optical Diagnostics and Sensing IX CY JAN 26-27, 2009 CL San Jose, CA SP SPIE AB During extra-vehicular activities (EVAs) or space walks astronauts over use their fingertips under pressure inside the confined spaces of gloves/space-suite. The repetitive hand motion is a probable cause for discomfort and injuries to the finger-tips. We describe a new wireless fiber-optic probe that can be integrated inside the astronaut glove for non-invasive blood perfusion measurements in distal finger tips. In this preliminary study, we present blood perfusion measurements while performing hand-grip exercises simulating the use of space tools. C1 [Ansari, Rafat R.] NASA, Glenn Res Ctr, Cleveland, OH 44035 USA. RP Ansari, RR (reprint author), NASA, Glenn Res Ctr, Cleveland, OH 44035 USA. EM Rafat.R.Ansari@nasa.gov RI Pollonini, Luca/J-9274-2014 OI Pollonini, Luca/0000-0003-2955-6355 NR 8 TC 0 Z9 0 U1 0 U2 1 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 978-0-8194-7432-2 J9 P SOC PHOTO-OPT INS PY 2009 VL 7186 AR 718609 DI 10.1117/12.809054 PG 9 WC Engineering, Biomedical; Remote Sensing; Optics SC Engineering; Remote Sensing; Optics GA BSS56 UT WOS:000285712100004 ER PT S AU Elsner, RF O'Dell, SL Ramsey, BD Weisskopf, MC AF Elsner, Ronald F. O'Dell, Stephen L. Ramsey, Brian D. Weisskopf, Martin C. BE O'Dell, SL Pareschi, G TI On the design of wide-field x-ray telescopes SO OPTICS FOR EUV, X-RAY, AND GAMMA-RAY ASTRONOMY IV SE Proceedings of SPIE LA English DT Proceedings Paper CT Conference on Optics for EUV, X-Ray, and Gamma-Ray Astronomy IV CY AUG 04-06, 2009 CL San Diego, CA SP SPIE DE X-ray astronomy; X-ray optics; ray trace; wide field-of-view optimization ID GRAZING-INCIDENCE OPTICS; OPTIMIZATION AB X-ray telescopes having a relatively wide field-of-view and spatial resolution vs. polar off-axis angle curves much flatter than the parabolic dependence characteristic of Wolter I designs are of great interest for surveys of the X-ray sky and potentially for study of the Sun's X-ray emission. We discuss the various considerations affecting the design of such telescopes, including the possible use of polynomial mirror surface prescriptions, a method of optimizing the polynomial coefficients, scaling laws for mirror segment length vs. intersection radius, the loss of on-axis spatial resolution, and the positioning of focal plane detectors. C1 [Elsner, Ronald F.; O'Dell, Stephen L.; Ramsey, Brian D.; Weisskopf, Martin C.] NASA Marshall Space Flight Ctr, Space Sci Off, Huntsville, AL 35812 USA. RP Elsner, RF (reprint author), NASA Marshall Space Flight Ctr, Space Sci Off, VP62, Huntsville, AL 35812 USA. EM ron.elsner@nasa.gov; steve.o'dell@nasa.gov; brian.ramsey@nasa.gov; martin@smoker.msfc.nasa.gov; steve.o'dell@nasa.gov NR 9 TC 0 Z9 0 U1 0 U2 0 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 978-0-8194-7727-9 J9 PROC SPIE PY 2009 VL 7437 AR 74370F DI 10.1117/12.831262 PG 12 WC Astronomy & Astrophysics; Optics SC Astronomy & Astrophysics; Optics GA BRX37 UT WOS:000283842600013 ER PT S AU Gubarev, MV O'Dell, SL Jones, WD Kester, TJ Griffith, CW Zhang, WW Saha, TT Chan, KW AF Gubarev, Mikhail V. O'Dell, Stephen L. Jones, William D. Kester, Thomas J. Griffith, Charles W. Zhang, William W. Saha, Timo T. Chan, Kai-Wing BE O'Dell, SL Pareschi, G TI A stainless-steel mandrel for slumping glass x-ray mirrors SO OPTICS FOR EUV, X-RAY, AND GAMMA-RAY ASTRONOMY IV SE Proceedings of SPIE LA English DT Proceedings Paper CT Conference on Optics for EUV, X-Ray, and Gamma-Ray Astronomy IV CY AUG 04-06, 2009 CL San Diego, CA SP SPIE DE mandrel fabrication; stainless-steel mandrels; metrology; x-ray mirrors; thermal forming ID OPTICS; MSFC AB We have fabricated a precision full-cylinder stainless-steel mandrel at NASA Marshall Space Flight Center. The mandrel is figured for a 30-cm-diameter primary (paraboloid) mirror of an 840-cm focal-length Wolter-1 telescope. We have developed this mandrel for experiments in slumping-thermal forming at about 600 degrees C-of glass mirror segments at NASA Goddard Space Flight Center, in support of NASA's participation in the International X-ray Observatory (IXO). Precision turning of stainless-steel mandrels may offer a low-cost alternative to conventional figuring of fused-silica or other glassy forming mandrels. We report on the fabrication, metrology, and performance of this first mandrel; then we discuss plans and goals for stainless-steel mandrel technology. C1 [Gubarev, Mikhail V.] NASA Marshall Space Flight Ctr, Space Sci Off, Huntsville, AL 35812 USA. RP Gubarev, MV (reprint author), NASA Marshall Space Flight Ctr, Space Sci Off, VP62, Huntsville, AL 35812 USA. EM mikhail.v.gubarev@nasa.gov OI O'Dell, Stephen/0000-0002-1868-8056 NR 24 TC 0 Z9 0 U1 0 U2 0 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 978-0-8194-7727-9 J9 PROC SPIE PY 2009 VL 7437 AR 74370Z DI 10.1117/12.831260 PG 12 WC Astronomy & Astrophysics; Optics SC Astronomy & Astrophysics; Optics GA BRX37 UT WOS:000283842600032 ER PT S AU Lehan, JP Atanossova, M Chan, KW Hadjimichael, T Saha, TT Hong, M Zhang, WW Blake, P AF Lehan, J. P. Atanossova, M. Chan, K. -W. Hadjimichael, T. Saha, T. T. Hong, M. Zhang, W. W. Blake, P. BE O'Dell, SL Pareschi, G TI Progress toward a complete metrology set for the International X-ray Observatory (IXO) soft x-ray mirrors SO OPTICS FOR EUV, X-RAY, AND GAMMA-RAY ASTRONOMY IV SE Proceedings of SPIE LA English DT Proceedings Paper CT Conference on Optics for EUV, X-Ray, and Gamma-Ray Astronomy IV CY AUG 04-06, 2009 CL San Diego, CA SP SPIE DE Optical metrology; x-ray optics; IXO AB We present an overview update of the metrologic approach to be employed for the segmented mirror fabrication for the IXO soft x-ray telescope. We compare results achieved to date with mission requirements. This is discussed in terms of inherent capability versus in-practice capability of the metrology. We find that all the needed metrology equipment are in hand but that a number of the needed quantities remain too uncertain relative to mission requirements. This is driven by the mounting of the mirrors themselves. We then discuss some plans for addressing the mirror mounting issues. Finally, we also briefly discuss some promising mandrel metrology techniques. C1 [Lehan, J. P.; Chan, K. -W.] NASA, Goddard Space Flight Ctr, Ctr Res & Explorat Space Sci & Technol, Baltimore, MD 21250 USA. RP Lehan, JP (reprint author), NASA, Goddard Space Flight Ctr, Ctr Res & Explorat Space Sci & Technol, 1000 Hilltop Circle, Baltimore, MD 21250 USA. NR 11 TC 1 Z9 1 U1 0 U2 0 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 978-0-8194-7727-9 J9 PROC SPIE PY 2009 VL 7437 AR 74370R DI 10.1117/12.826625 PG 9 WC Astronomy & Astrophysics; Optics SC Astronomy & Astrophysics; Optics GA BRX37 UT WOS:000283842600024 ER PT S AU Zhang, WW AF Zhang, William W. BE O'Dell, SL Pareschi, G TI Manufacture of Mirror Glass Substrates for The NUSTAR Mission SO OPTICS FOR EUV, X-RAY, AND GAMMA-RAY ASTRONOMY IV SE Proceedings of SPIE LA English DT Proceedings Paper CT Conference on Optics for EUV, X-Ray, and Gamma-Ray Astronomy IV CY AUG 04-06, 2009 CL San Diego, CA SP SPIE DE X-ray optics; lightweight optics; NuSTAR; Glass Slumping AB The NuSTAR (Nuclear Spectroscopy Telescope Array) observatory (Harrison et al. 2009), expected to be launched into an equatorial low earth orbit in 2011, will have two mirror assemblies capable of imaging X-rays in the hard X-ray band between 5 keV and 80 keV. It will be the first X-ray observatory using multilayer coatings to significantly expand the bandwidth of the typical X-ray telescope of 0.1 keV to 10 keV. The mirror assemblies use a segmented design to simplify the construction process, as such they require 4,680 mirror substrates coated with appropriately designed multilayers to enhance reflectivity for hard X-rays. These substrates are produced by slumping commercially available thin glass sheets. In this paper we report on our work of manufacturing these substrates at NASA Goddard Space Flight Center. C1 NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Zhang, WW (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. NR 4 TC 13 Z9 13 U1 1 U2 1 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 978-0-8194-7727-9 J9 PROC SPIE PY 2009 VL 7437 AR 74370N DI 10.1117/12.830225 PG 11 WC Astronomy & Astrophysics; Optics SC Astronomy & Astrophysics; Optics GA BRX37 UT WOS:000283842600021 ER PT S AU Gizon, L Schunker, H Baldner, CS Basu, S Birch, AC Bogart, RS Braun, DC Cameron, R Duvall, TL Hanasoge, SM Jackiewicz, J Roth, M Stahn, T Thompson, MJ Zharkov, S AF Gizon, L. Schunker, H. Baldner, C. S. Basu, S. Birch, A. C. Bogart, R. S. Braun, D. C. Cameron, R. Duvall, T. L., Jr. Hanasoge, S. M. Jackiewicz, J. Roth, M. Stahn, T. Thompson, M. J. Zharkov, S. BE Thompson, MJ Balogh, A Culhane, JL Nordlund, A Solanki, SK Zahn, JP TI Helioseismology of Sunspots: A Case Study of NOAA Region 9787 SO ORIGIN AND DYNAMICS OF SOLAR MAGNETISM SE Space Science Series of ISSI LA English DT Article; Book Chapter DE Sun; Sunspots; Helioseismology ID TIME-DISTANCE HELIOSEISMOLOGY; RING-DIAGRAM ANALYSIS; SOLAR ACTIVE REGIONS; MODE TRAVEL-TIMES; LOCAL HELIOSEISMOLOGY; WAVE-PROPAGATION; SOUND SPEED; P-MODES; FLOWS; INVERSION AB Various methods of helioseismology are used to study the subsurface properties of the Sunspot in NOAA Active Region 9787. This sunspot was chosen because it is axisymmetric, shows little evolution during 20-28 January 2002, and was observed continuously by the MDI/SOHO instrument. AR 9787 is visible on helioseismic maps of the farside of the Sun from 15 January, i.e. days before it crossed the East limb. Oscillations have reduced amplitudes in the sunspot at all frequencies, whereas a region of enhanced acoustic power above 5.5 mHz (above the quiet-Sun acoustic cutoff) is seen outside the sunspot and the plage region. This enhanced acoustic power has been Suggested to be caused by the conversion of acoustic waves into magneto-acoustic waves that are refracted back into the interior and re-emerge as acoustic waves in the quiet Sun. Observations show that the sunspot absorbs a significant fraction of the incoming p and f modes around 3 mHz. A numerical simulation of MHD wave propagation through a simple model of AR 9787 confirmed that wave absorption is likely to be due to the partial conversion of incoming waves into magneto-acoustic waves that propagate down the sunspot. Wave travel times and mode frequencies are affected by the sunspot. In most cases, wave packets that propagate through the sunspot have reduced travel times. At short travel distances, however, the sign of the travel-time shifts appears to depend sensitively on how the data are processed and, in particular, on filtering in frequency-wavenumber space. We carry out two linear inversions for wave speed: one using travel-times and phase-speed filters and the other one using mode frequencies from ring analysis. These two inversions give subsurface wave-speed profiles with opposite signs and different amplitudes. The travel-time measurements also imply different subsurface flow patterns in the surface layer depending on the filtering procedure that is used. Current sensitivity kernels are unable to reconcile these measurements, perhaps because they rely on imperfect models of the power spectrum of solar oscillations. We present a linear inversion for flows of ridge-filtered travel times. This inversion shows a horizontal outflow in the upper 4 Mill that is consistent with the moat flow deduced from the surface motion of moving magnetic features. From this study of AR 9787, we conclude that we are currently unable to provide a unified description of the subsurface structure and dynamics of the sunspot. C1 [Gizon, L.; Schunker, H.; Cameron, R.; Jackiewicz, J.; Roth, M.; Stahn, T.] Max Planck Inst Sonnensyst Forsch, D-37191 Katlenburg Lindau, Germany. [Baldner, C. S.; Basu, S.] Yale Univ, Dept Astron, New Haven, CT 06520 USA. [Birch, A. C.; Braun, D. C.] Colorado Res Associates, Boulder, CO 80301 USA. [Bogart, R. S.; Hanasoge, S. M.] Stanford Univ, Hansen Expt Phys Lab, Stanford, CA 94305 USA. [Duvall, T. L., Jr.] NASA, Goddard Space Flight Ctr, Lab Solar Phys, Greenbelt, MD 20771 USA. [Thompson, M. J.; Zharkov, S.] Univ Sheffield, Sch Math & Stat, Sheffield S3 7RH, S Yorkshire, England. RP Gizon, L (reprint author), Max Planck Inst Sonnensyst Forsch, D-37191 Katlenburg Lindau, Germany. EM gizon@mps.mpg.de RI Basu, Sarbani/B-8015-2014 OI Basu, Sarbani/0000-0002-6163-3472 NR 65 TC 0 Z9 0 U1 0 U2 0 PU SPRINGER PI NEW YORK PA 233 SPRING STREET, NEW YORK, NY 10013, UNITED STATES SN 1385-7525 BN 978-1-4419-0238-2 J9 SPACE SCI SER ISSI PY 2009 VL 32 BP 249 EP 273 DI 10.1007/978-1-4419-0239-9_15 D2 10.1007/978-1-4419-0239-9 PG 25 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BKH57 UT WOS:000268118700015 ER PT S AU Hathaway, DH AF Hathaway, David H. BE Thompson, MJ Balogh, A Culhane, JL Nordlund, A Solanki, SK Zahn, JP TI Solar Cycle Forecasting SO ORIGIN AND DYNAMICS OF SOLAR MAGNETISM SE Space Science Series of ISSI LA English DT Article; Book Chapter DE Solar activity; Sunspot cycle; Solar cycle forecasting ID FLUX; AMPLITUDE; DYNAMO; MINIMUM; MODELS; FIELD; SIZE AB Predicting the behavior of a solar cycle after it is well underway (2-3 years after minimum) can be done with a fair degree of skill using auto-regression and curve fitting techniques that don't require any knowledge of the physics involved. Predicting the amplitude of a solar cycle near, or before, the time of solar cycle minimum can be done using precursors such as geomagnetic activity and polar fields that do have some connection to the physics but the connections are uncertain and the precursors provide less reliable forecasts. Predictions for the amplitude of cycle 24 using these precursor techniques give drastically different values. Recently, dynamo models have been used directly with assimilated data to predict the amplitude of sunspot cycle 24 but have also given significantly different predictions. While others have questioned both the predictability of the solar cycle and the ability of current dynamo models to provide predictions, it is clear that cycle 24 will help to discriminate between some opposing dynamo models. C1 NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA. RP Hathaway, DH (reprint author), NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA. EM David.Hathaway@nasa.gov NR 35 TC 0 Z9 0 U1 0 U2 0 PU SPRINGER PI NEW YORK PA 233 SPRING STREET, NEW YORK, NY 10013, UNITED STATES SN 1385-7525 BN 978-1-4419-0238-2 J9 SPACE SCI SER ISSI PY 2009 VL 32 BP 401 EP 412 DI 10.1007/978-1-4419-0239-9_20 D2 10.1007/978-1-4419-0239-9 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BKH57 UT WOS:000268118700020 ER PT S AU Lawson, PW AF Lawson, Peter W. BE Knudsen, EE Michael, JH TI What Are We Missing? Butterflies, Flowers, and Salmon Models SO PACIFIC SALMON ENVIRONMENTAL AND LIFE HISTORY MODELS: ADVANCING SCIENCE FOR SUSTAINABLE SALMON IN THE FUTURE SE American Fisheries Society Symposium LA English DT Proceedings Paper CT Symposium on Pacific Salmon Environmental and Life History Models CY SEP 13-14, 2005 CL Anchorage, AK SP Amer Fisheries Soc ID NORTHEAST PACIFIC; SURVIVAL RATES; DYNAMICS; OREGON; PATTERNS AB We understand our environment through our senses and tend to interpret the behavior of other animals in the context of the world we understand. Butterflies and flowers sometimes show distinctive patterns in ultraviolet light that are important to them but invisible to us. Likewise, the senses of fish and their experience of the world are very different from ours. Many aspects of a salmon's environment, such as olfactory stimuli, are completely invisible to us. Other factors, like certain aspects of habitat alteration, are visible but unnoticed because they occurred gradually or long ago. Like Poe's purloined letter they are cryptic-there for us to see if we only knew what to look for. As we build salmon models we base them on what we understand is important to the fish. However, our anthropocentric bias may cause us to overlook or misinterpret factors of importance. In addition, our necessarily simplified models, when applied to management, may result in a pernicious simplification of the salmon populations we wish to preserve. For example, if we model and manage for a dominant (or highly visible or easily monitored) salmon life history we may inadvertently eliminate other life histories of equal importance, or reduce diversity in ways that affect population viability. We should actively seek to identify important factors missing from our models and be aware of critical assumptions. Recognizing that our models are tools used to understand and manage salmon, we should try to understand the broader implications of these models to the future of the salmon we hope to preserve. In this essay, I offer speculation about what we may be missing in freshwater habitat, life history diversity, metapopulation dynamics, ocean survival, and water chemistry. I also consider the question of scale, and the effect our philosophical viewpoint may have on the direction and application of our modeling efforts and the likelihood of successful outcomes. C1 Natl Marine Fisheries Serv, Newport Res Stn, Newport, OR 97365 USA. RP Lawson, PW (reprint author), Natl Marine Fisheries Serv, Newport Res Stn, 2032 SE OSU Dr, Newport, OR 97365 USA. EM peter.w.lawson@noaa.gov NR 25 TC 1 Z9 1 U1 1 U2 1 PU AMER FISHERIES SOC PI BETHESDA PA 5410 GROSVENOR LANE, STE 110, BETHESDA, MD 20814-2199 USA SN 0892-2284 BN 978-1-934874-09-7 J9 AM FISH S S PY 2009 VL 71 BP 33 EP 44 PG 12 WC Fisheries SC Fisheries GA BLY21 UT WOS:000271411600003 ER PT S AU Munoz-Mari, J Plaza, AJ Gualtieri, JA Camps-Valls, G AF Munoz-Mari, Jordi Plaza, Antonio J. Gualtieri, J. Anthony Camps-Valls, Gustavo BE Xhafa, F TI Parallel Implementations of SVM for Earth Observation SO PARALLEL PROGRAMMING, MODELS AND APPLICATIONS IN GRID AND P2P SYSTEMS SE Advances in Parallel Computing LA English DT Article; Book Chapter DE Parallel processing; image classification; remote sensing; support vector machine; multispectral; hyperspectral; kernel methods ID HYPERSPECTRAL IMAGE CLASSIFICATION; SUPPORT VECTOR MACHINES; CLUSTER; WORKSTATIONS; OPTIMIZATION; ALGORITHMS; NETWORKS AB Imaging spectroscopy, also known as hyperspectral remote sensing, is concerned with the measurement, analysis, and interpretation of spectra acquired from a given scene (or specific object) at a short, medium or long distance by an airborne or satellite sensor. Analysis in a timely manner of the acquired multidimensional images allows to develop applications with high social impact, such as urban growing monitoring, crop fields identification, target detection for military and defense/security deployment, wildland fire detection and monitoring, biological threat detection, biophysical parameter estimation, or monitoring of oil spills and other types of chemical contamination. In this context, support vector machines (SVM) [1, 2, 3] have become one of the state-of-the-art machine learning tools for hyperspectral image classification. However, its high computational cost for large scale applications makes the use of SVM limited to off-line processing scenarios. Certainly, with the recent explosion in the amount and complexity of hyperspectral data, parallel processing has soon become a requirement in many remote sensing missions, especially with the advent of low-cost systems such as commodity clusters and distributed networks of computers In order to address this relevant issue, this chapter explores the development of two parallel versions of SVMs for remote sensing image classification. Sequential minimal optimization is a very popular algorithm for training SVMs, but it still requires a large amount of computation time for solving large size problems. In this work, we evaluate the performance of a parallel implementation of the SVM based on the parallelization of the incomplete Cholesky factorization and present novel parallel implementations that balance the load across the available processors through standard Master-Worker decompositions. Both methodologies are theoretically analyzed in terms of scalability, computational efficiency and time response. The impact of the multi-class scheme is also analyzed. Results on real multispectral and hyperspectral datasets illustrate the performance of the methods. We finally discuss the possibility of obtaining processing results quickly enough for practical use via the Marenostrum supercomputer available at the Barcelona Supercomputing Center in Spain, and other massively parallel facilities at NASA's Goddard Space Flight Center in Maryland. C1 [Munoz-Mari, Jordi; Camps-Valls, Gustavo] Univ Valencia, IPL, Dept Elect Engn, E-46003 Valencia, Spain. [Plaza, Antonio J.] Univ Extremadura, Dept Comp Sci, Caceres, Spain. [Gualtieri, J. Anthony] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Munoz-Mari, J (reprint author), Univ Valencia, IPL, Dept Elect Engn, E-46003 Valencia, Spain. EM jordi@uv.es; aplaza@unex.es; Anthony.Gualtieri@gst.com; gcamps@uv.es OI Munoz-Mari, Jordi/0000-0002-3014-3921; Plaza, Antonio/0000-0002-9613-1659 NR 60 TC 8 Z9 8 U1 0 U2 2 PU IOS PRESS PI AMSTERDAM PA NIEUWE HEMWEG 6B, 1013 BG AMSTERDAM, NETHERLANDS SN 0927-5452 BN 978-1-60750-004-9 J9 ADV PARALLEL COMPUT PY 2009 VL 17 BP 292 EP 312 DI 10.3233/978-1-60750-004-9-292 PG 21 WC Computer Science, Hardware & Architecture SC Computer Science GA BMB00 UT WOS:000271713700012 ER PT J AU Watson, AB Ahumada, AJ AF Watson, A. B. Ahumada, A. J., Jr. TI The image-based acuity model: A general model for image recognition SO PERCEPTION LA English DT Meeting Abstract C1 [Watson, A. B.; Ahumada, A. J., Jr.] NASA, Human Syst Integrat Div, Ames Res Ctr, Washington, DC USA. EM andrew.b.watson@nasa.gov NR 0 TC 0 Z9 0 U1 0 U2 1 PU PION LTD PI LONDON PA 207 BRONDESBURY PARK, LONDON NW2 5JN, ENGLAND SN 0301-0066 J9 PERCEPTION JI Perception PY 2009 VL 38 SU S BP 60 EP 61 PG 2 WC Ophthalmology; Psychology; Psychology, Experimental SC Ophthalmology; Psychology GA V16YN UT WOS:000207905000196 ER PT J AU Mortensen, DH Bech, S Begault, DR Adelstein, BD AF Mortensen, Ditte H. Bech, Soren Begault, Durand R. Adelstein, Bernard D. TI The relative importance of visual, auditory, and haptic information for the user's experience of mechanical switches SO PERCEPTION LA English DT Article ID FEEDBACK; ILLUSIONS; TACTILE AB While the use of hand tools and other everyday manually controlled devices is naturally accompanied by multisensory feedback, the deployment of fully multimodal virtual interfaces requires that haptic, acoustic, and visual cues be synthesised. The complexity and character of this synthesis will depend on a thorough understanding of the multimodal perceptual experience, including the interrelations between the individual sensory channels during manual interaction. In this study seventy participants were asked to rank the manual operation of ten electromechanical switches according to preference. The participants were randomly assigned in groups of ten to one of seven sensory presentation conditions. These conditions comprised six bit-nodal and unimodal sensory combinations created by selectively restricting the flow of haptic, auditory, and visual information, plus one condition in which ful sensory information was available. A principal components analysis on the obtained ranking data indicated that the sensory conditions with unimpeded haptic information were clearly distinct from those in which the haptic cues were impeded. The analysis also showed that, for switch use, the unimodal haptic condition most closely approached the condition with combined haptic, auditory, and visual feedback, compared with all of the conditions where haptic feedback was restricted. C1 [Mortensen, Ditte H.; Bech, Soren] Bang & Olufsen As, Struer, Denmark. [Begault, Durand R.; Adelstein, Bernard D.] NASA, Ames Res Ctr, Human Syst Integrat Div, Moffett Field, CA 94035 USA. RP Mortensen, DH (reprint author), Bang & Olufsen As, Peter Bangs Vej 15, Struer, Denmark. EM dhm@bang-olufsen.dk RI Bech, Soren/L-4070-2015 OI Bech, Soren/0000-0002-0924-1914 NR 23 TC 1 Z9 1 U1 3 U2 7 PU PION LTD PI LONDON PA 207 BRONDESBURY PARK, LONDON NW2 5JN, ENGLAND SN 0301-0066 J9 PERCEPTION JI Perception PY 2009 VL 38 IS 10 BP 1560 EP 1571 DI 10.1068/p5929 PG 12 WC Ophthalmology; Psychology; Psychology, Experimental SC Ophthalmology; Psychology GA 533WC UT WOS:000272855100011 PM 19950486 ER PT B AU Tunstel, E Dolan, JM Fong, T Schreckenghost, D AF Tunstel, Edward Dolan, John M. Fong, Terrence Schreckenghost, Debra BE Madhavan, R Tubstel, E Messina, E TI Mobile Robotic Surveying Performance for Planetary Surface Site Characterization SO PERFORMANCE EVALUATION AND BENCHMARKING OF INTELLIGENT SYSTEMS LA English DT Proceedings Paper CT Workshop on Performance Metrics for Intelligent Systems (PerMIS 08) CY AUG 19-21, 2008 CL Natl Inst Stand, Gaithersburg, MD HO Natl Inst Stand AB Robotic systems will perform mobile surveys for scientific and engineering purposes as part of future missions on lunar and planetary surfaces. With site characterization as a task objective various system configurations and surveying techniques are possible. This chapter describes several examples of mobile surveying approaches using local and remote sensing configurations. A geometric measure of area coverage performance is applied to each and relative performance in surveying a common area is characterized by expected performance trends. Performance metrics that solely express geometric aspects of the robotic task are limited in utility as decision aids to human mission operators. As such, the importance of enriching such metrics by incorporating additional attributes germane to surveying on planetary surfaces is highlighted. Examples of enriched metrics employed by recent NASA research work on human-supervised robotic surveying are provided. C1 [Tunstel, Edward] Johns Hopkins Univ, Appl Phys Lab, Dept Space, Johns Hopkins Rd, Laurel, MD 20723 USA. [Dolan, John M.] Carnegie Mellon Univ, Inst Robot, Pittsburgh, PA 15213 USA. [Fong, Terrence] NASA Ames Res Ctr, Intelligent Robot Grp, Moffett Field, CA 94035 USA. [Schreckenghost, Debra] TRACLabs Inc, Webster, NY USA. RP Tunstel, E (reprint author), Johns Hopkins Univ, Appl Phys Lab, Dept Space, Johns Hopkins Rd, Laurel, MD 20723 USA. EM edward.tunstel@jhuapl.edu; jmd@cs.cmu.edu; terry.fong@nasa.gov; schreck@traclabs.com FU NASA Astrobiology Science and Technology Instrument Development; NASA Exploration Systems Technology Development Program under the "Human-Robotic Systems" NASA Small Business Innovative Research(SBIR) program; NASA Small Business Innovative Research(SBIR) FX We thank Hans Utz, Tod Milam, David Lees, and Matt Deans for assisting with the development and implementation of real-time robot performance monitoring. This work was partially supported by the NASA Astrobiology Science and Technology Instrument Development program, the NASA Exploration Systems Technology Development Program under the Human-Robotic Systems project and the NASA Small Business Innovative Research(SBIR) program. NR 23 TC 0 Z9 0 U1 0 U2 1 PU SPRINGER PI NEW YORK PA 233 SPRING STREET, NEW YORK, NY 10013, UNITED STATES BN 978-1-4419-0491-1 PY 2009 BP 249 EP + DI 10.1007/978-1-4419-0492-8_11 PG 3 WC Computer Science, Artificial Intelligence SC Computer Science GA BMM54 UT WOS:000272813500011 ER PT S AU Peterson, N Anusuya-Rangappa, L Shirazi, BA Song, WZ Huang, RJ Tran, D Chien, S LaHusen, R AF Peterson, Nina Anusuya-Rangappa, Lohith Shirazi, Behrooz A. Song, WenZhan Huang, Renjie Tran, Daniel Chien, Steve LaHusen, Rick BE Hassanien, AE Abawajy, JH Abraham, A Hagras, H TI Volcano Monitoring: A Case Study in Pervasive Computing SO PERVASIVE COMPUTING: INNOVATIONS IN INTELLIGENT MULTIMEDIA AND APPLICATIONS SE Computer Communications and Networks Series LA English DT Article; Book Chapter DE Wireless sensor networks; Pervasive computing; Environment monitoring; Quality of service; Situation awareness AB Recent advances in wireless sensor network technology have provided robust and reliable solutions for sophisticated pervasive computing applications such as inhospitable terrain environmental monitoring. We present a case study for developing a real-time pervasive computing system, called OASIS for optimized autonomous space in situ sensor-web, which combines ground assets (a sensor network) and space assets (NASA's earth observing (EO-1) satellite) to monitor volcanic activities at Mount St. Helens. OASIS's primary goals are: to integrate complementary space and in situ ground sensors into an interactive and autonomous sensorweb, to optimize power and communication resource management of the sensorweb and to provide mechanisms for seamless and scalable fusion of future space and in situ components. The OASIS in situ ground sensor network development addresses issues related to power management, bandwidth management, quality of service management, topology and routing management, and test-bed design. The space segment development consists of EO-1 architectural enhancements, feedback of EO-1 data into the in situ component, command and control integration, data ingestion and dissemination and field demonstrations. C1 [Peterson, Nina; Anusuya-Rangappa, Lohith; Shirazi, Behrooz A.; Huang, Renjie] Washington State Univ, Sch Elect Engn & Comp Sci, Pullman, WA 99163 USA. [LaHusen, Rick] USGS Cascades Volcano Observ, Vancouver, WA 98660 USA. [Tran, Daniel; Chien, Steve] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Song, WenZhan] Washington State Univ, Sch Elect Engn & Comp Sci, Vancouver, WA 98686 USA. RP Peterson, N (reprint author), Washington State Univ, Sch Elect Engn & Comp Sci, Pullman, WA 99163 USA. EM npicone@eecs.wsu.edu NR 29 TC 4 Z9 4 U1 0 U2 1 PU SPRINGER-VERLAG LONDON LTD PI GODALMING PA SWEETAPPLE HOUSE CATTESHALL RD FARNCOMBE, GODALMING GU7 1NH, SURREY, ENGLAND SN 1617-7975 BN 978-1-84882-598-7 J9 COMPUT COMMUN NETW S PY 2009 BP 201 EP 230 DI 10.1007/978-1-84882-599-4_10 PG 30 WC Computer Science, Artificial Intelligence; Computer Science, Hardware & Architecture SC Computer Science GA BLT76 UT WOS:000270992400010 ER PT J AU Pissulla, D Seckmeyer, G Cordero, RR Blumthaler, M Schallhart, B Webb, A Kift, R Smedley, A Bais, AF Kouremeti, N Cede, A Herman, J Kowalewskig, M AF Pissulla, D. Seckmeyer, G. Cordero, R. R. Blumthaler, M. Schallhart, B. Webb, A. Kift, R. Smedley, A. Bais, A. F. Kouremeti, N. Cede, A. Herman, J. Kowalewskig, M. TI Comparison of atmospheric spectral radiance measurements from five independently calibrated systems SO PHOTOCHEMICAL & PHOTOBIOLOGICAL SCIENCES LA English DT Article ID SKY RADIANCE; IRRADIANCE; SPECTRORADIOMETERS; SENSITIVITY; UNCERTAINTY; ULTRAVIOLET AB A variety of instruments have been developed over the past 50 years to measure spectral radiance in absolute units at UV and visible wavelengths with high spectral resolution. While there is considerable experience in the measurement of spectral irradiance, less emphasis has been given to the reliable measurement of spectral radiance from ground observations. We discuss the methodology and calibration procedures for five instruments capable of making such measurements. Four of these instruments are based on double monochromators that scan each wavelength in turn, and one is based on a single monochromator with a charged coupled device (CCD) allowing the recording of all wavelengths simultaneously. The measured spectral radiance deviates between 3% and about 35% depending on the instruments. The results are compared with radiative transfer calculations when the aerosol characteristics of the atmosphere are known. C1 [Pissulla, D.; Seckmeyer, G.] Leibniz Univ Hannover, Inst Meteorol & Climatol, Hannover, Germany. [Cordero, R. R.] Univ Tecn Feder Santa Maria, Valparaiso, Chile. [Cordero, R. R.] Univ Santiago Chile, Santiago, Chile. [Blumthaler, M.; Schallhart, B.] Innsbruck Med Univ, Div Biomed Phys, Innsbruck, Austria. [Blumthaler, M.; Schallhart, B.] Univ Manchester, Sch Earth Atmospher & Environm Sci, Manchester M13 9PL, Lancs, England. [Bais, A. F.; Kouremeti, N.] Aristotle Univ Thessaloniki, Lab Atmospher Phys, Thessaloniki, Greece. [Cede, A.; Herman, J.; Kowalewskig, M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Pissulla, D (reprint author), Leibniz Univ Hannover, Inst Meteorol & Climatol, Hannover, Germany. EM Pissulla@muk.uni-hannover.de RI Bais, Alkiviadis/D-2230-2009; Smedley, Andrew/N-9865-2014; OI Bais, Alkiviadis/0000-0003-3899-2001; Smedley, Andrew/0000-0001-7137-6628; Herman, Jay/0000-0002-9146-1632; Kift, Richard/0000-0003-1826-3653 FU WMO FX Part of this study has been conducted in the framework of the EC Integrated Project SCOUT-O3 (contract 505390-GOCE-CT2004). We would like to thank WMO for providing financial support to groups taking part in the Izana campaign. Furthermore, we are indebted to the director of the Izana Observatory, Dr Emilio Cuevas for providing the facilities to host the campaign and to Alberto Redondas for his continuous support during the campaign. NR 35 TC 13 Z9 13 U1 0 U2 5 PU ROYAL SOC CHEMISTRY PI CAMBRIDGE PA THOMAS GRAHAM HOUSE, SCIENCE PARK, MILTON RD, CAMBRIDGE CB4 0WF, CAMBS, ENGLAND SN 1474-905X EI 1474-9092 J9 PHOTOCH PHOTOBIO SCI JI Photochem. Photobiol. Sci. PY 2009 VL 8 IS 4 BP 516 EP 527 DI 10.1039/b817018e PG 12 WC Biochemistry & Molecular Biology; Biophysics; Chemistry, Physical SC Biochemistry & Molecular Biology; Biophysics; Chemistry GA 426ZI UT WOS:000264747000012 PM 19337666 ER PT J AU Boykin, TB Kharche, N Klimeck, G AF Boykin, Timothy B. Kharche, Neerav Klimeck, Gerhard TI Non-primitive rectangular cells for tight-binding electronic structure calculations SO PHYSICA E-LOW-DIMENSIONAL SYSTEMS & NANOSTRUCTURES LA English DT Article DE Brillouin zone; Allowed wavevectors; Zone unfolding AB Rectangular non-primitive unit cells are computationally convenient for use in nanodevice electronic structure and transport calculations. When these cells are used for Calculations of structures with periodicity, the resulting bands are zone-folded and must be unfolded in order to identify important gaps and masses. Before the zone-unfolding method can be applied, one must first determine the allowed wavevectors for the specific non-primitive cell. Because most computationally convenient non-primitive cells do not have axes parallel to the primitive cell direct lattice vectors, finding the allowed wavevectors is generally a non-trivial task. (Solid state texts generally treat only the simplest case in which the non-primitive and primitive cell axes are all aligned.) Rectangular non-primitive cells with one axis aligned along a specific direction are especially useful for obtaining the approximate random-alloy bands for a bulk crystal, a critical verification step in any randorn-alloy nanostructure calculation. Here, we present an easily implemented method for determining a non-primitive rectangular cell for the FCC lattice with an axis aligned in a desired direction and the associated allowed primitive cell wavevectors. We illustrate its use by unfolding the bands of Ge. (C) 2008 Elsevier B.V. All rights reserved. C1 [Boykin, Timothy B.] Univ Alabama, Dept Elect & Comp Engn, Huntsville, AL 35899 USA. [Kharche, Neerav; Klimeck, Gerhard] Purdue Univ, Network Computat Nanotechnol, Sch Elect & Comp Engn, W Lafayette, IN 47907 USA. [Klimeck, Gerhard] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Boykin, TB (reprint author), Univ Alabama, Dept Elect & Comp Engn, Huntsville, AL 35899 USA. EM boykin@ece.uah.edu RI Kharche, Neerav/F-4331-2015; Klimeck, Gerhard/A-1414-2012 OI Kharche, Neerav/0000-0003-1014-6022; Klimeck, Gerhard/0000-0001-7128-773X FU Semiconductor Research Corporation; National Science Foundation FX This work was supported by Semiconductor Research Corporation. The work described in this publication was carried out in part at the jet Propulsion Laboratory, California Institute of Technology under a contract with the National Aeronautics and Space Administration, and jet Propulsion Laboratory. nanohub.org Computational resources provided by the Network for Computational Nanotechnology, funded by the National Science Foundation were used. NR 14 TC 11 Z9 11 U1 0 U2 2 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 1386-9477 J9 PHYSICA E JI Physica E PD JAN PY 2009 VL 41 IS 3 BP 490 EP 494 DI 10.1016/j.physe.2008.09.022 PG 5 WC Nanoscience & Nanotechnology; Physics, Condensed Matter SC Science & Technology - Other Topics; Physics GA 402LR UT WOS:000263015700032 ER PT J AU Shaw, MD Schneiderman, JF Bueno, J Palmer, BS Delsing, P Echternach, PM AF Shaw, M. D. Schneiderman, J. F. Bueno, J. Palmer, B. S. Delsing, P. Echternach, P. M. TI Characterization of an entangled system of two superconducting qubits using a multiplexed capacitance measurement SO PHYSICAL REVIEW B LA English DT Article DE capacitors; Cooper pairs; ground states; information theory; quantum computing; quantum entanglement ID CHARGE QUBITS; QUANTUM STATE; CAVITY AB We characterize a pair of Cooper-pair boxes coupled with a fixed capacitor using spectroscopy and measurements of the ground-state quantum capacitance. We use the extracted parameters to estimate the concurrence or degree of entanglement between the two qubits. We also present a thorough demonstration of a multiplexed quantum capacitance measurement technique, which is in principle scalable to a large array of superconducting qubits. C1 [Shaw, M. D.; Schneiderman, J. F.; Echternach, P. M.] Univ So Calif, Dept Phys & Astron, Los Angeles, CA 90089 USA. [Schneiderman, J. F.; Delsing, P.] Chalmers, S-41296 Gothenburg, Sweden. [Bueno, J.; Delsing, P.; Echternach, P. M.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Palmer, B. S.] Lab Phys Sci, College Pk, MD 20740 USA. RP Shaw, MD (reprint author), Univ So Calif, Dept Phys & Astron, Los Angeles, CA 90089 USA. RI Delsing, Per/F-7288-2010; Schneiderman, Justin/D-4508-2013 OI Delsing, Per/0000-0002-1222-3506; Schneiderman, Justin/0000-0002-4441-2360 FU National Security Agency; NASA; University of Southern California College of Arts and Sciences FX We would like to thank Richard Muller for performing the electron-beam lithography. This work was conducted at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration (NASA), and was funded by a grant from the National Security Agency. J.B. acknowledges support from NASA. M. S. acknowledges support from the University of Southern California College of Arts and Sciences. NR 25 TC 7 Z9 7 U1 0 U2 1 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 JAN PY 2009 VL 79 IS 1 AR 014516 DI 10.1103/PhysRevB.79.014516 PG 8 WC Physics, Condensed Matter SC Physics GA 401XX UT WOS:000262977900104 ER PT J AU Abbott, B Abbott, R Adhikari, R Ajith, P Allen, B Allen, G Amin, R Anderson, DP Anderson, SB Anderson, WG Arain, MA Araya, M Armandula, H Armor, P Aso, Y Aston, S Aufmuth, P Aulbert, C Babak, S Ballmer, S Bantilan, H Barish, BC Barker, C Barker, D Barr, B Barriga, P Barton, MA Bastarrika, M Bayer, K Betzwieser, J Beyersdorf, PT Bilenko, IA Billingsley, G Biswas, R Black, E Blackburn, K Blackburn, L Blair, D Bland, B Bodiya, TP Bogue, L Bork, R Boschi, V Bose, S Brady, PR Braginsky, VB Brau, JE Brinkmann, M Brooks, A Brown, DA Brunet, G Bullington, A Buonanno, A Burmeister, O Byer, RL Cadonati, L Cagnoli, G Camp, JB Cannizzo, J Cannon, K Cao, J Cardenas, L Casebolt, T Castaldi, G Cepeda, C Chalkley, E Charlton, P Chatterji, S Chelkowski, S Chen, Y Christensen, N Clark, D Clark, J Cokelaer, T Conte, R Cook, D Corbitt, T Coyne, D Creighton, JDE Creighton, TD Cumming, A Cunningham, L Cutler, RM Dalrymple, J Danzmann, K Davies, G DeBra, D Degallaix, J Degree, M Dergachev, V Desai, S DeSalvo, R Dhurandhar, S Diaz, M Dickson, J Dietz, A Donovan, F Dooley, KL Doomes, EE Drever, RWP Duke, I Dumas, JC Dupuis, RJ Dwyer, JG Echols, C Effler, A Ehrens, P Ely, G Espinoza, E Etzel, T Evans, T Fairhurst, S Fan, Y Fazi, D Fehrmann, H Fejer, MM Finn, LS Flasch, K Fotopoulos, N Freise, A Frey, R Fricke, T Fritschel, P Frolov, VV Fyffe, M Garofoli, J Gholami, I Giaime, JA Giampanis, S Giardina, KD Goda, K Goetz, E Goggin, L Gonzalez, G Gossler, S Gouaty, R Grant, A Gras, S Gray, C Gray, M Greenhalgh, RJS Gretarsson, AM Grimaldi, F Grosso, R Grote, H Grunewald, S Guenther, M Gustafson, EK Gustafson, R Hage, B Hallam, JM Hammer, D Hanna, C Hanson, J Harms, J Harry, G Harstad, E Hayama, K Hayler, T Heefner, J Heng, IS Hennessy, M Heptonstall, A Hewitson, M Hild, S Hirose, E Hoak, D Hosken, D Hough, J Huttner, SH Ingram, D Ito, M Ivanov, A Johnson, B Johnson, WW Jones, DI Jones, G Jones, R Ju, L Kalmus, P Kalogera, V Kamat, S Kanner, J Kasprzyk, D Katsavounidis, E Kawabe, K Kawamura, S Kawazoe, F Kells, W Keppel, DG Khalili, FY Khan, R Khazanov, E Kim, C King, P Kissel, JS Klimenko, S Kokeyama, K Kondrashov, V Kopparapu, RK Kozak, D Kozhevatov, I Krishnan, B Kwee, P Lam, PK Landry, M Lang, MM Lantz, B Lazzarini, A Lei, M Leindecker, N Leonhardt, V Leonor, I Libbrecht, K Lin, H Lindquist, P Lockerbie, NA Lodhia, D Lormand, M Lu, P Lubinski, M Lucianetti, A Luck, H Machenschalk, B MacInnis, M Mageswaran, M Mailand, K Mandic, V Marka, S Marka, Z Markosyan, A Markowitz, J Maros, E Martin, I Martin, RM Marx, JN Mason, K Matichard, F Matone, L Matzner, R Mavalvala, N McCarthy, R McClelland, DE McGuire, SC McHugh, M McIntyre, G McIvor, G McKechan, D McKenzie, K Meier, T Melissinos, A Mendell, G Mercer, RA Meshkov, S Messenger, CJ Meyers, D Miller, J Minelli, J Mitra, S Mitrofanov, VP Mitselmakher, G Mittleman, R Miyakawa, O Moe, B Mohanty, S Moreno, G Mossavi, K MowLowry, C Mueller, G Mukherjee, S Mukhopadhyay, H Muller-Ebhardt, H Munch, J Murray, P Myers, E Myers, J Nash, T Nelson, J Newton, G Nishizawa, A Numata, K O'Dell, J Ogin, G O'Reilly, B O'Shaughnessy, R Ottaway, DJ Ottens, RS Overmier, H Owen, BJ Pan, Y Pankow, C Papa, MA Parameshwaraiah, V Patel, P Pedraza, M Penn, S Perreca, A Petrie, T Pinto, IM Pitkin, M Pletsch, HJ Plissi, MV Postiglione, F Principe, M Prix, R Quetschke, V Raab, F Rabeling, DS Radkins, H Rainer, N Rakhmanov, M Ramsunder, M Rehbein, H Reid, S Reitze, DH Riesen, R Riles, K Rivera, B Robertson, NA Robinson, C Robinson, EL Roddy, S Rodriguez, A Rogan, AM Rollins, J Romano, JD Romie, J Route, R Rowan, S Rudiger, A Ruet, L Russell, P Ryan, K Sakata, S Samidi, M de la Jordana, LS Sandberg, V Sannibale, V Saraf, S Sarin, P Sathyaprakash, BS Sato, S Saulson, PR Savage, R Savov, P Schediwy, SW Schilling, R Schnabel, R Schofield, R Schutz, BF Schwinberg, P Scott, SM Searle, AC Sears, B Seifert, F Sellers, D Sengupta, AS Shawhan, P Shoemaker, DH Sibley, A Siemens, X Sigg, D Sinha, S Sintes, AM Slagmolen, BJJ Slutsky, J Smith, JR Smith, MR Smith, ND Somiya, K Sorazu, B Stein, LC Stochino, A Stone, R Strain, KA Strom, DM Stuver, A Summerscales, TZ Sun, KX Sung, M Sutton, PJ Takahashi, H Tanner, DB Taylor, R Taylor, R Thacker, J Thorne, KA Thorne, KS Thuring, A Tokmakov, KV Torres, C Torrie, C Traylor, G Trias, M Tyler, W Ugolini, D Ulmen, J Urbanek, K Vahlbruch, H Van Den Broeck, C van der Sluys, M Vass, S Vaulin, R Vecchio, A Veitch, J Veitch, P Vigeland, S Villar, A Vorvick, C Vyachanin, SP Waldman, SJ Wallace, L Ward, H Ward, R Weinert, M Weinstein, A Weiss, R Wen, S Wette, K Whelan, JT Whitbeck, DM Whitcomb, SE Whiting, BF Wilkinson, C Willems, PA Williams, HR Williams, L Willke, B Wilmut, I Winkler, W Wipf, CC Wiseman, AG Woan, G Wooley, R Worden, J Wu, W Yakushin, I Yamamoto, H Yan, Z Yoshida, S Zanolin, M Zhang, J Zhang, L Zhao, C Zotov, N Zucker, M Zweizig, J AF Abbott, B. Abbott, R. Adhikari, R. Ajith, P. Allen, B. Allen, G. Amin, R. Anderson, D. P. Anderson, S. B. Anderson, W. G. Arain, M. A. Araya, M. Armandula, H. Armor, P. Aso, Y. Aston, S. Aufmuth, P. Aulbert, C. Babak, S. Ballmer, S. Bantilan, H. Barish, B. C. Barker, C. Barker, D. Barr, B. Barriga, P. Barton, M. A. Bastarrika, M. Bayer, K. Betzwieser, J. Beyersdorf, P. T. Bilenko, I. A. Billingsley, G. Biswas, R. Black, E. Blackburn, K. Blackburn, L. Blair, D. Bland, B. Bodiya, T. P. Bogue, L. Bork, R. Boschi, V. Bose, S. Brady, P. R. Braginsky, V. B. Brau, J. E. Brinkmann, M. Brooks, A. Brown, D. A. Brunet, G. Bullington, A. Buonanno, A. Burmeister, O. Byer, R. L. Cadonati, L. Cagnoli, G. Camp, J. B. Cannizzo, J. Cannon, K. Cao, J. Cardenas, L. Casebolt, T. Castaldi, G. Cepeda, C. Chalkley, E. Charlton, P. Chatterji, S. Chelkowski, S. Chen, Y. Christensen, N. Clark, D. Clark, J. Cokelaer, T. Conte, R. Cook, D. Corbitt, T. Coyne, D. Creighton, J. D. E. Creighton, T. D. Cumming, A. Cunningham, L. Cutler, R. M. Dalrymple, J. Danzmann, K. Davies, G. DeBra, D. Degallaix, J. Degree, M. Dergachev, V. Desai, S. DeSalvo, R. Dhurandhar, S. Diaz, M. Dickson, J. Dietz, A. Donovan, F. Dooley, K. L. Doomes, E. E. Drever, R. W. P. Duke, I. Dumas, J.-C. Dupuis, R. J. Dwyer, J. G. Echols, C. Effler, A. Ehrens, P. Ely, G. Espinoza, E. Etzel, T. Evans, T. Fairhurst, S. Fan, Y. Fazi, D. Fehrmann, H. Fejer, M. M. Finn, L. S. Flasch, K. Fotopoulos, N. Freise, A. Frey, R. Fricke, T. Fritschel, P. Frolov, V. V. Fyffe, M. Garofoli, J. Gholami, I. Giaime, J. A. Giampanis, S. Giardina, K. D. Goda, K. Goetz, E. Goggin, L. Gonzalez, G. Gossler, S. Gouaty, R. Grant, A. Gras, S. Gray, C. Gray, M. Greenhalgh, R. J. S. Gretarsson, A. M. Grimaldi, F. Grosso, R. Grote, H. Grunewald, S. Guenther, M. Gustafson, E. K. Gustafson, R. Hage, B. Hallam, J. M. Hammer, D. Hanna, C. Hanson, J. Harms, J. Harry, G. Harstad, E. Hayama, K. Hayler, T. Heefner, J. Heng, I. S. Hennessy, M. Heptonstall, A. Hewitson, M. Hild, S. Hirose, E. Hoak, D. Hosken, D. Hough, J. Huttner, S. H. Ingram, D. Ito, M. Ivanov, A. Johnson, B. Johnson, W. W. Jones, D. I. Jones, G. Jones, R. Ju, L. Kalmus, P. Kalogera, V. Kamat, S. Kanner, J. Kasprzyk, D. Katsavounidis, E. Kawabe, K. Kawamura, S. Kawazoe, F. Kells, W. Keppel, D. G. Khalili, F. Ya. Khan, R. Khazanov, E. Kim, C. King, P. Kissel, J. S. Klimenko, S. Kokeyama, K. Kondrashov, V. Kopparapu, R. K. Kozak, D. Kozhevatov, I. Krishnan, B. Kwee, P. Lam, P. K. Landry, M. Lang, M. M. Lantz, B. Lazzarini, A. Lei, M. Leindecker, N. Leonhardt, V. Leonor, I. Libbrecht, K. Lin, H. Lindquist, P. Lockerbie, N. A. Lodhia, D. Lormand, M. Lu, P. Lubinski, M. Lucianetti, A. Lueck, H. Machenschalk, B. MacInnis, M. Mageswaran, M. Mailand, K. Mandic, V. Marka, S. Marka, Z. Markosyan, A. Markowitz, J. Maros, E. Martin, I. Martin, R. M. Marx, J. N. Mason, K. Matichard, F. Matone, L. Matzner, R. Mavalvala, N. McCarthy, R. McClelland, D. E. McGuire, S. C. McHugh, M. McIntyre, G. McIvor, G. McKechan, D. McKenzie, K. Meier, T. Melissinos, A. Mendell, G. Mercer, R. A. Meshkov, S. Messenger, C. J. Meyers, D. Miller, J. Minelli, J. Mitra, S. Mitrofanov, V. P. Mitselmakher, G. Mittleman, R. Miyakawa, O. Moe, B. Mohanty, S. Moreno, G. Mossavi, K. MowLowry, C. Mueller, G. Mukherjee, S. Mukhopadhyay, H. Mueller-Ebhardt, H. Munch, J. Murray, P. Myers, E. Myers, J. Nash, T. Nelson, J. Newton, G. Nishizawa, A. Numata, K. O'Dell, J. Ogin, G. O'Reilly, B. O'Shaughnessy, R. Ottaway, D. J. Ottens, R. S. Overmier, H. Owen, B. J. Pan, Y. Pankow, C. Papa, M. A. Parameshwaraiah, V. Patel, P. Pedraza, M. Penn, S. Perreca, A. Petrie, T. Pinto, I. M. Pitkin, M. Pletsch, H. J. Plissi, M. V. Postiglione, F. Principe, M. Prix, R. Quetschke, V. Raab, F. Rabeling, D. S. Radkins, H. Rainer, N. Rakhmanov, M. Ramsunder, M. Rehbein, H. Reid, S. Reitze, D. H. Riesen, R. Riles, K. Rivera, B. Robertson, N. A. Robinson, C. Robinson, E. L. Roddy, S. Rodriguez, A. Rogan, A. M. Rollins, J. Romano, J. D. Romie, J. Route, R. Rowan, S. Ruediger, A. Ruet, L. Russell, P. Ryan, K. Sakata, S. Samidi, M. de la Jordana, L. Sancho Sandberg, V. Sannibale, V. Saraf, S. Sarin, P. Sathyaprakash, B. S. Sato, S. Saulson, P. R. Savage, R. Savov, P. Schediwy, S. W. Schilling, R. Schnabel, R. Schofield, R. Schutz, B. F. Schwinberg, P. Scott, S. M. Searle, A. C. Sears, B. Seifert, F. Sellers, D. Sengupta, A. S. Shawhan, P. Shoemaker, D. H. Sibley, A. Siemens, X. Sigg, D. Sinha, S. Sintes, A. M. Slagmolen, B. J. J. Slutsky, J. Smith, J. R. Smith, M. R. Smith, N. D. Somiya, K. Sorazu, B. Stein, L. C. Stochino, A. Stone, R. Strain, K. A. Strom, D. M. Stuver, A. Summerscales, T. Z. Sun, K.-X. Sung, M. Sutton, P. J. Takahashi, H. Tanner, D. B. Taylor, R. Taylor, R. Thacker, J. Thorne, K. A. Thorne, K. S. Thuering, A. Tokmakov, K. V. Torres, C. Torrie, C. Traylor, G. Trias, M. Tyler, W. Ugolini, D. Ulmen, J. Urbanek, K. Vahlbruch, H. Van Den Broeck, C. van der Sluys, M. Vass, S. Vaulin, R. Vecchio, A. Veitch, J. Veitch, P. Vigeland, S. Villar, A. Vorvick, C. Vyachanin, S. P. Waldman, S. J. Wallace, L. Ward, H. Ward, R. Weinert, M. Weinstein, A. Weiss, R. Wen, S. Wette, K. Whelan, J. T. Whitbeck, D. M. Whitcomb, S. E. Whiting, B. F. Wilkinson, C. Willems, P. A. Williams, H. R. Williams, L. Willke, B. Wilmut, I. Winkler, W. Wipf, C. C. Wiseman, A. G. Woan, G. Wooley, R. Worden, J. Wu, W. Yakushin, I. Yamamoto, H. Yan, Z. Yoshida, S. Zanolin, M. Zhang, J. Zhang, L. Zhao, C. Zotov, N. Zucker, M. Zweizig, J. CA LIGO Sci Collaboration TI Einstein@Home search for periodic gravitational waves in LIGO S4 data SO PHYSICAL REVIEW D LA English DT Article ID PRECESSING NEUTRON-STARS; INSPIRALING BINARIES; RADIATION; TEMPLATES AB A search for periodic gravitational waves, from sources such as isolated rapidly spinning neutron stars, was carried out using 510 h of data from the fourth LIGO science run (S4). The search was for quasimonochromatic waves in the frequency range from 50 to 1500 Hz, with a linear frequency drift f (measured at the solar system barycenter) in the range -f/tau < f < 0.1f/tau, where the minimum spin-down age tau was 1000 yr for signals below 300 Hz and 10 000 yr above 300 Hz. The main computational work of the search was distributed over approximately 100 000 computers volunteered by the general public. This large computing power allowed the use of a relatively long coherent integration time of 30 h, despite the large parameter space searched. No statistically significant signals were found. The sensitivity of the search is estimated, along with the fraction of parameter space that was vetoed because of contamination by instrumental artifacts. In the 100 to 200 Hz band, more than 90% of sources with dimensionless gravitational-wave strain amplitude greater than 10(-23) would have been detected. C1 [Babak, S.; Chen, Y.; Degallaix, J.; Gholami, I.; Grunewald, S.; Krishnan, B.; Papa, M. A.; Schutz, B. F.; Sintes, A. M.; Somiya, K.; Takahashi, H.; Whelan, J. T.] Max Planck Inst Gravitat Phys, Albert Einstein Inst, D-14476 Golm, Germany. [Allen, B.; Aulbert, C.; Brinkmann, M.; Burmeister, O.; Danzmann, K.; Fehrmann, H.; Gossler, S.; Grote, H.; Harms, J.; Hewitson, M.; Lueck, H.; Machenschalk, B.; Messenger, C. J.; Mossavi, K.; Mueller-Ebhardt, H.; Pletsch, H. J.; Prix, R.; Rainer, N.; Rehbein, H.; Ruediger, A.; Schilling, R.; Schnabel, R.; Seifert, F.; Weinert, M.; Willke, B.; Winkler, W.] Max Planck Inst Gravitat Phys, Albert Einstein Inst, D-30167 Hannover, Germany. [Summerscales, T. Z.] Andrews Univ, Berrien Springs, MI 49104 USA. [Dickson, J.; Gray, M.; Lam, P. K.; McClelland, D. E.; McKenzie, K.; MowLowry, C.; Rabeling, D. S.; Searle, A. C.; Slagmolen, B. J. J.; Wette, K.] Australian Natl Univ, Canberra, ACT 0200, Australia. [Drever, R. W. P.] CALTECH, Pasadena, CA 91125 USA. [Savov, P.; Thorne, K. S.] Caltech CaRT, Pasadena, CA 91125 USA. [Cokelaer, T.; Davies, G.; Dietz, A.; Fairhurst, S.; Jones, G.; McKechan, D.; Robinson, C.; Sathyaprakash, B. S.; Sutton, P. J.; Van Den Broeck, C.] Cardiff Univ, Cardiff CF24 3AA, Wales. [Bantilan, H.; Christensen, N.; Ely, G.; Vigeland, S.] Carleton Coll, Northfield, MN 55057 USA. [Charlton, P.] Charles Sturt Univ, Wagga Wagga, NSW 2678, Australia. [Aso, Y.; Dwyer, J. G.; Kalmus, P.; Kamat, S.; Khan, R.; Marka, S.; Marka, Z.; Matone, L.; Rollins, J.] Columbia Univ, New York, NY 10027 USA. [Gretarsson, A. M.; Zanolin, M.] Embry Riddle Aeronaut Univ, Prescott, AZ 86301 USA. [Penn, S.] Hobart & William Smith Coll, Geneva, NY 14456 USA. [Khazanov, E.; Kozhevatov, I.] Russian Acad Sci, Inst Appl Phys, Nizhnii Novgorod 603950, Russia. [Dhurandhar, S.; Mitra, S.; Mukhopadhyay, H.] Inter Univ Ctr Astron & Astrophys, Pune 411007, Maharashtra, India. [Aufmuth, P.; Danzmann, K.; Hage, B.; Kwee, P.; Lueck, H.; Meier, T.; Thuering, A.; Vahlbruch, H.; Willke, B.] Leibniz Univ Hannover, D-30167 Hannover, Germany. [Abbott, B.; Abbott, R.; Adhikari, R.; Anderson, S. B.; Araya, M.; Armandula, H.; Ballmer, S.; Barish, B. C.; Betzwieser, J.; Billingsley, G.; Black, E.; Blackburn, K.; Bork, R.; Boschi, V.; Brooks, A.; Cannon, K.; Cardenas, L.; Cepeda, C.; Chatterji, S.; Coyne, D.; DeSalvo, R.; Dupuis, R. J.; Echols, C.; Ehrens, P.; Espinoza, E.; Etzel, T.; Fazi, D.; Fricke, T.; Goggin, L.; Gustafson, E. K.; Heefner, J.; Ivanov, A.; Kells, W.; Keppel, D. G.; King, P.; Kondrashov, V.; Kozak, D.; Lazzarini, A.; Lei, M.; Libbrecht, K.; Lindquist, P.; Mageswaran, M.; Mailand, K.; Maros, E.; Marx, J. N.; McIntyre, G.; Meshkov, S.; Meyers, D.; Miller, J.; Miyakawa, O.; Nash, T.; Ogin, G.; Patel, P.; Pedraza, M.; Robertson, N. A.; Russell, P.; Samidi, M.; Sannibale, V.; Sears, B.; Sengupta, A. S.; Smith, M. R.; Stochino, A.; Taylor, R.; Tyler, W.; Vass, S.; Villar, A.; Waldman, S. J.; Wallace, L.; Ward, R.; Weinstein, A.; Whitcomb, S. E.; Willems, P. A.; Yamamoto, H.; Zhang, L.; Zweizig, J.] CALTECH, LIGO, Pasadena, CA 91125 USA. [Bayer, K.; Blackburn, L.; Bodiya, T. P.; Brunet, G.; Cao, J.; Corbitt, T.; Donovan, F.; Duke, I.; Fritschel, P.; Goda, K.; Grimaldi, F.; Harry, G.; Katsavounidis, E.; MacInnis, M.; Markowitz, J.; Mason, K.; Mavalvala, N.; Mittleman, R.; Ottaway, D. J.; Ruet, L.; Sarin, P.; Shoemaker, D. H.; Smith, N. D.; Stein, L. C.; Weiss, R.; Wipf, C. C.; Zucker, M.] MIT, LIGO, Cambridge, MA 02139 USA. [Barker, C.; Barker, D.; Bland, B.; Cook, D.; Effler, A.; Garofoli, J.; Gray, C.; Guenther, M.; Ingram, D.; Johnson, B.; Kawabe, K.; Landry, M.; Lubinski, M.; McCarthy, R.; Mendell, G.; Moreno, G.; Myers, E.; Myers, J.; Parameshwaraiah, V.; Raab, F.; Radkins, H.; Rivera, B.; Ryan, K.; Sandberg, V.; Savage, R.; Schwinberg, P.; Sigg, D.; Vorvick, C.; Wilkinson, C.; Worden, J.] LIGO Hanford Observ, Richland, WA 99325 USA. [Bogue, L.; Evans, T.; Frolov, V. V.; Fyffe, M.; Giaime, J. A.; Giardina, K. D.; Hanson, J.; Hoak, D.; Lormand, M.; O'Reilly, B.; Overmier, H.; Riesen, R.; Roddy, S.; Romie, J.; Sellers, D.; Sibley, A.; Stuver, A.; Thacker, J.; Torres, C.; Wooley, R.; Yakushin, I.] LIGO Livingston Observ, Livingston, LA 70754 USA. [Amin, R.; Giaime, J. A.; Gonzalez, G.; Gouaty, R.; Hanna, C.; Johnson, W. W.; Kissel, J. S.; Matichard, F.; Rodriguez, A.; Slutsky, J.; Sung, M.; Wen, S.] Louisiana State Univ, Baton Rouge, LA 70803 USA. [Zotov, N.] Louisiana Tech Univ, Ruston, LA 71272 USA. 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L.; Casebolt, T.; Clark, D.; DeBra, D.; Degree, M.; Fejer, M. M.; Hennessy, M.; Lantz, B.; Leindecker, N.; Lu, P.; Markosyan, A.; Route, R.; Sinha, S.; Sun, K.-X.; Ulmen, J.; Urbanek, K.] Stanford Univ, Stanford, CA 94305 USA. [Brown, D. A.; Dalrymple, J.; Hirose, E.; Saulson, P. R.; Smith, J. R.] Syracuse Univ, Syracuse, NY 13244 USA. [Desai, S.; Finn, L. S.; Kopparapu, R. K.; Lang, M. M.; Minelli, J.; O'Shaughnessy, R.; Owen, B. J.; Petrie, T.; Ramsunder, M.; Thorne, K. A.; Whitbeck, D. M.; Williams, H. R.] Penn State Univ, University Pk, PA 16802 USA. [Matzner, R.; McIvor, G.] Univ Texas Austin, Austin, TX 78712 USA. [Creighton, T. D.; Diaz, M.; Grosso, R.; Hayama, K.; Mohanty, S.; Mukherjee, S.; Romano, J. D.; Stone, R.] Univ Texas Brownsville & Texas Southmost Coll, Brownsville, TX 78520 USA. [Ugolini, D.] Trinity Univ, San Antonio, TX 78212 USA. [de la Jordana, L. Sancho; Sintes, A. M.; Trias, M.] Univ Illes Balears, E-07122 Palma de Mallorca, Spain. [Hosken, D.; Munch, J.; Veitch, P.] Univ Adelaide, Adelaide, SA 5005, Australia. [Aston, S.; Chelkowski, S.; Cutler, R. M.; Freise, A.; Hallam, J. M.; Hild, S.; Kasprzyk, D.; Lodhia, D.; Perreca, A.; Robinson, E. L.; Vecchio, A.; Veitch, J.] Univ Birmingham, Birmingham B15 2TT, W Midlands, England. [Anderson, D. P.] Univ Calif Berkeley, Berkeley, CA 94720 USA. [Arain, M. A.; Dooley, K. L.; Klimenko, S.; Lin, H.; Lucianetti, A.; Martin, R. M.; Mercer, R. A.; Mitselmakher, G.; Mueller, G.; Ottens, R. S.; Pankow, C.; Quetschke, V.; Reitze, D. H.; Tanner, D. B.; Whiting, B. F.; Williams, L.; Wu, W.] Univ Florida, Gainesville, FL 32611 USA. [Barr, B.; Barton, M. A.; Bastarrika, M.; Cagnoli, G.; Chalkley, E.; Clark, J.; Cumming, A.; Cunningham, L.; Grant, A.; Heng, I. S.; Heptonstall, A.; Hough, J.; Huttner, S. H.; Jones, R.; Martin, I.; Miller, J.; Murray, P.; Nelson, J.; Newton, G.; Pitkin, M.; Plissi, M. V.; Reid, S.; Robertson, N. A.; Rowan, S.; Sorazu, B.; Strain, K. A.; Taylor, R.; Tokmakov, K. V.; Torrie, C.; Traylor, G.; Ward, H.; Woan, G.] Univ Glasgow, Glasgow G12 8QQ, Lanark, Scotland. [Buonanno, A.; Kanner, J.; Pan, Y.; Shawhan, P.] Univ Maryland, College Pk, MD 20742 USA. [Cadonati, L.] Univ Massachusetts, Amherst, MA 01003 USA. [Dergachev, V.; Goetz, E.; Gustafson, R.; Riles, K.; Zhang, J.] Univ Michigan, Ann Arbor, MI 48109 USA. [Brau, J. E.; Frey, R.; Harstad, E.; Ito, M.; Leonor, I.; Schofield, R.; Strom, D. M.] Univ Oregon, Eugene, OR 97403 USA. [Mandic, V.] Univ Minnesota, Minneapolis, MN 55455 USA. [Fricke, T.; Giampanis, S.; Melissinos, A.] Univ Rochester, Rochester, NY 14627 USA. [Conte, R.; Postiglione, F.] Univ Salerno, I-84084 Fisciano, Salerno, Italy. [Castaldi, G.; Pinto, I. M.; Principe, M.] Univ Sannio Benevento, I-82100 Benevento, Italy. [Jones, D. I.] Univ Southampton, Southampton SO17 1BJ, Hants, England. [Lockerbie, N. A.] Univ Strathclyde, Glasgow G1 1XQ, Lanark, Scotland. [Barriga, P.; Blair, D.; Dumas, J.-C.; Fan, Y.; Gras, S.; Ju, L.; Schediwy, S. W.; Yan, Z.; Zhao, C.] Univ Western Australia, Nedlands, WA 6009, Australia. [Allen, B.; Anderson, W. G.; Armor, P.; Biswas, R.; Brady, P. R.; Creighton, J. D. E.; Flasch, K.; Fotopoulos, N.; Hammer, D.; Moe, B.; Papa, M. A.; Siemens, X.; Vaulin, R.; Wiseman, A. G.] Univ Wisconsin, Milwaukee, WI 53201 USA. [Bose, S.; Rogan, A. M.] Washington State Univ, Pullman, WA 99164 USA. RP Abbott, B (reprint author), Max Planck Inst Gravitat Phys, Albert Einstein Inst, D-14476 Golm, Germany. RI Biswas, Rahul/H-7474-2016; Khalili, Farit/D-8113-2012; Vecchio, Alberto/F-8310-2015; Mow-Lowry, Conor/F-8843-2015; Khan, Rubab/F-9455-2015; Ottaway, David/J-5908-2015; Postiglione, Fabio/O-4744-2015; Sigg, Daniel/I-4308-2015; Pinto, Innocenzo/L-3520-2016; Harms, Jan/J-4359-2012; Frey, Raymond/E-2830-2016; Ward, Robert/I-8032-2014; Finn, Lee Samuel/A-3452-2009; Mitrofanov, Valery/D-8501-2012; Bilenko, Igor/D-5172-2012; Allen, Bruce/K-2327-2012; Chen, Yanbei/A-2604-2013; Barker, David/A-5671-2013; Fricke, Thomas/B-6885-2013; Zhao, Chunnong/C-2403-2013; Ju, Li/C-2623-2013; Pitkin, Matthew/I-3802-2013; Vyatchanin, Sergey/J-2238-2012; Khazanov, Efim/B-6643-2014; Lucianetti, Antonio/G-7383-2014; Martin, Iain/A-2445-2010; Hild, Stefan/A-3864-2010; Schutz, Bernard/B-1504-2010; Rowan, Sheila/E-3032-2010; Strain, Kenneth/D-5236-2011; Raab, Frederick/E-2222-2011; Lueck, Harald/F-7100-2011; Kawazoe, Fumiko/F-7700-2011; Freise, Andreas/F-8892-2011; Kawabe, Keita/G-9840-2011; Barriga, Pablo/A-3929-2008; Lam, Ping Koy/A-5276-2008; McClelland, David/E-6765-2010 OI Nishizawa, Atsushi/0000-0003-3562-0990; Zweizig, John/0000-0002-1521-3397; O'Shaughnessy, Richard/0000-0001-5832-8517; Freise, Andreas/0000-0001-6586-9901; Whiting, Bernard F/0000-0002-8501-8669; Principe, Maria/0000-0002-6327-0628; Kanner, Jonah/0000-0001-8115-0577; Whelan, John/0000-0001-5710-6576; Fairhurst, Stephen/0000-0001-8480-1961; Boschi, Valerio/0000-0001-8665-2293; Matichard, Fabrice/0000-0001-8982-8418; Pinto, Innocenzo M./0000-0002-2679-4457; Minelli, Jeff/0000-0002-5330-912X; Hallam, Jonathan Mark/0000-0002-7087-0461; Biswas, Rahul/0000-0002-0774-8906; Sorazu, Borja/0000-0002-6178-3198; Stuver, Amber/0000-0003-0324-5735; Vecchio, Alberto/0000-0002-6254-1617; Khan, Rubab/0000-0001-5100-5168; Postiglione, Fabio/0000-0003-0628-3796; Sigg, Daniel/0000-0003-4606-6526; Frey, Raymond/0000-0003-0341-2636; Stein, Leo/0000-0001-7559-9597; Ward, Robert/0000-0001-5503-5241; Finn, Lee Samuel/0000-0002-3937-0688; Allen, Bruce/0000-0003-4285-6256; Zhao, Chunnong/0000-0001-5825-2401; Pitkin, Matthew/0000-0003-4548-526X; Strain, Kenneth/0000-0002-2066-5355; Lueck, Harald/0000-0001-9350-4846; Lam, Ping Koy/0000-0002-4421-601X; McClelland, David/0000-0001-6210-5842 NR 48 TC 56 Z9 56 U1 2 U2 12 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 JAN PY 2009 VL 79 IS 2 AR 022001 DI 10.1103/PhysRevD.79.022001 PG 29 WC Astronomy & Astrophysics; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA 401YK UT WOS:000262979800005 ER PT J AU Abers, ES Bhatia, AK Dicus, DA Repko, WW Rosenbaum, DC Teplitz, VL AF Abers, E. S. Bhatia, A. K. Dicus, D. A. Repko, W. W. Rosenbaum, D. C. Teplitz, V. L. TI Charges on strange quark nuggets in space SO PHYSICAL REVIEW D LA English DT Article ID COLOR SUPERCONDUCTIVITY; E(+)E(-) EMISSION; MATTER SURFACES; STARS; NUCLEARITES; RADIATION AB Since Witten's seminal 1984 paper on the subject, searches for evidence of strange quark nuggets (SQNs) have proven unsuccessful. In the absence of experimental evidence ruling out SQNs, the validity of theories introducing mechanisms that increase their stability should continue to be tested. To stimulate electromagnetic SQN searches, particularly space searches, we estimate the net charge that would develop on a SQN in space exposed to various radiation baths (and showers) capable of liberating the SQN's less strongly bound electrons, taking into account recombination with ambient electrons. We consider, in particular, the cosmic microwave background, radiation from the sun, and diffuse galactic and extragalactic ultraviolet backgrounds. The largest charge, for the settings considered, develops on a solar system SQN exposed to a solar X-ray flare. A possible dramatic signal of SQNs in explosive astrophysical events is noted. C1 [Abers, E. S.] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA. [Bhatia, A. K.; Teplitz, V. L.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Dicus, D. A.] Univ Texas Austin, Dept Phys, Austin, TX 78712 USA. [Repko, W. W.] Michigan State Univ, Dept Phys & Astron, E Lansing, MI 48824 USA. [Rosenbaum, D. C.; Teplitz, V. L.] So Methodist Univ, Dept Phys, Dallas, TX 75275 USA. RP Abers, ES (reprint author), Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA. FU U. S. Department of Energy [DE-FG03-93ER40757]; National Science Foundation [PHY-0555544] FX L. T. very much appreciates a number of very helpful conversations with Demos Kazanas, one with Floyd Stecker on Ref. [ 23] and one with M. Alford on the effects of Cooper pairing. Dr. Alford kindly provided a number of very helpful comments on the first version of this paper. D. C. R. and V. L. T. are also grateful to Jonathan Gardner for calling SN-2006gy to our attention, as well as C. Kilbourne for talking WHIM with us. D. A. D. was supported in part by the U. S. Department of Energy under Grant No. DE-FG03-93ER40757. W. W. R. was supported in part by the National Science Foundation under Grant PHY-0555544. NR 54 TC 3 Z9 3 U1 0 U2 0 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 1550-7998 J9 PHYS REV D JI Phys. Rev. D PD JAN PY 2009 VL 79 IS 2 AR 023513 DI 10.1103/PhysRevD.79.023513 PG 11 WC Astronomy & Astrophysics; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA 401YK UT WOS:000262979800023 ER PT J AU Mikellides, IG AF Mikellides, Ioannis G. TI Effects of viscosity in a partially ionized channel flow with thermionic emission SO PHYSICS OF PLASMAS LA English DT Article DE channel flow; plasma collision processes; plasma flow; plasma simulation; thermionic emission; viscosity ID HOLLOW-CATHODE; MODEL AB The flow of the partially ionized gas inside thermionic hollow cathodes spans a diverse range of theoretical disciplines in plasma physics and fluid mechanics. Understanding and predicting the evolution of such flows has many practical implications because hollow cathodes are critical components of electric propulsion systems used onboard scientific and commercial spacecraft presently in space or in the mission planning stages. As space missions become more demanding of the propulsion system in terms of throughput, understanding and predicting failure mechanisms of the system becomes imperative. Two-dimensional numerical simulations of the partially ionized gas generated by a thermionic hollow cathode have been performed to quantify the effects of viscosity inside the cylindrical channel of the device. A comparison of the inviscid and fully viscous flow fields shows that viscosity has a significant impact on the atomic species and a lesser effect on the ions. The internal pressure is determined to be more than 40% higher compared to the inviscid solution and the Reynolds number for the flow of atoms is found to be less than 20 inside the channel. Although the Mach number is computed to be < 0.1 for approximately 95% of the channel, the solution for the velocity flow field begins to deviate from the Poiseuille (parabolic) solution at about 50% of the channel due mainly to collisional drag with ions. C1 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. NR 23 TC 6 Z9 6 U1 2 U2 6 PU AMER INST PHYSICS PI MELVILLE PA 1305 WALT WHITMAN RD, STE 300, MELVILLE, NY 11747-4501 USA SN 1070-664X EI 1089-7674 J9 PHYS PLASMAS JI Phys. Plasmas PD JAN PY 2009 VL 16 IS 1 AR 013501 DI 10.1063/1.3056397 PG 10 WC Physics, Fluids & Plasmas SC Physics GA 401UM UT WOS:000262967900035 ER PT S AU Lansbergen, GP Rahman, R Caro, J Collaert, N Biesemans, S Klimeck, G Hollenberg, LCL Rogge, S AF Lansbergen, G. P. Rahman, R. Caro, J. Collaert, N. Biesemans, S. Klimeck, G. Hollenberg, L. C. L. Rogge, S. BE Caldas, MJ Studart, N TI +Level Spectrum Of Single Gated As Donors SO PHYSICS OF SEMICONDUCTORS SE AIP Conference Proceedings LA English DT Proceedings Paper CT 29th International Conference on Physics of Semiconductors CY JUL 27-AUG 01, 2008 CL Rio de Janeiro, BRAZIL DE Single donors; FinFET; Transport spectroscopy ID SILICON; STATE AB We study the electrical transport through single As donors incorporated in the channel of a FinFET, i.e. a donor in a three-terminal geometry. By means of spectroscopic measurements in conjuction with a NEMO-3D model, we can identify the excited states and associate them with either the donors Coulomb potential, a triangular well at the interface or a hybridized combination of the two. The correspondence between the transport measurements, the theoretical model and the local environment provides an atomic understanding of actual gated donors in a nanostructure. C1 [Lansbergen, G. P.; Caro, J.; Rogge, S.] Delft Univ Technol, Kavli Inst Nanosci, Lorentzweg 1, NL-2628 CJ Delft, Netherlands. [Rahman, R.; Klimeck, G.] Purdue Univ, Network Computat Nanotechnol, W Lafayette, IN 47907 USA. [Hollenberg, L. C. L.] Univ Melbourne, Ctr Quantum Comp Technol, Sch Phys, Melbourne, Vic 3010, Australia. [Collaert, N.; Biesemans, S.] IMEC, B-3001 Heverlee, Belgium. [Klimeck, G.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Lansbergen, GP (reprint author), Delft Univ Technol, Kavli Inst Nanosci, Lorentzweg 1, NL-2628 CJ Delft, Netherlands. RI Hollenberg, Lloyd/B-2296-2010; Klimeck, Gerhard/A-1414-2012; Rogge, Sven/G-3709-2010; OI Klimeck, Gerhard/0000-0001-7128-773X; Rahman, Rajib/0000-0003-1649-823X NR 13 TC 0 Z9 0 U1 0 U2 0 PU AMER INST PHYSICS PI MELVILLE PA 2 HUNTINGTON QUADRANGLE, STE 1NO1, MELVILLE, NY 11747-4501 USA SN 0094-243X BN 978-0-7354-0736-7 J9 AIP CONF PROC PY 2009 VL 1199 BP 93 EP + PG 2 WC Engineering, Electrical & Electronic; Physics, Applied SC Engineering; Physics GA BQR10 UT WOS:000281590800044 ER PT J AU Turyshev, SG AF Turyshev, S. G. TI Experimental tests of general relativity: recent progress and future directions SO PHYSICS-USPEKHI LA English DT Review ID INVERSE-SQUARE LAW; SOLAR GRAVITATIONAL DEFLECTION; PREFERRED-FRAME THEORIES; FINE-STRUCTURE CONSTANT; PROBE WMAP OBSERVATIONS; ANGULAR POWER SPECTRUM; LASER ASTROMETRIC TEST; ATOMIC CLOCK ENSEMBLE; NEWLY RECOVERED DATA; SPACE-TIME FRAME AB Einstein's general theory of relativity is the standard theory of gravity, especially where the needs of astronomy, astrophysics, cosmology, and fundamental physics are concerned. As such, this theory is used for many practical purposes involving spacecraft navigation, geodesy, and time transfer. We review the foundations of general relativity, discuss recent progress in tests of relativistic gravity, and present motivations for the new generation of high-accuracy tests of new physics beyond general relativity. Space-based experiments in fundamental physics are presently capable of uniquely addressing important questions related to the fundamental laws of nature. We discuss the advances in our understanding of fundamental physics that are anticipated in the near future and evaluate the discovery potential of a number of recently proposed space-based gravitational experiments. C1 [Turyshev, S. G.] Moscow MV Lomonosov State Univ, Sternberg Astron Inst, Moscow 119992, Russia. [Turyshev, S. G.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Turyshev, SG (reprint author), Moscow MV Lomonosov State Univ, Sternberg Astron Inst, Univ Prosp 13, Moscow 119992, Russia. EM turyshev@jpl.nasa.gov NR 476 TC 36 Z9 38 U1 0 U2 10 PU TURPION LTD PI BRISTOL PA C/O TURPION LTD, IOP PUBLISHING, TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6HG, ENGLAND SN 1063-7869 EI 1468-4780 J9 PHYS-USP+ JI Phys. Usp. PD JAN PY 2009 VL 52 IS 1 BP 1 EP 27 DI 10.3367/UFNe.0179.200901a.0003 PG 27 WC Physics, Multidisciplinary SC Physics GA 454US UT WOS:000266708800001 ER PT J AU Halekas, JS Delory, GT Lin, RP Stubbs, TJ Farrell, WM AF Halekas, J. S. Delory, G. T. Lin, R. P. Stubbs, T. J. Farrell, W. M. TI Lunar Prospector measurements of secondary electron emission from lunar regolith SO PLANETARY AND SPACE SCIENCE LA English DT Article DE Moon; Surface charging; Secondary electron emission; Lunar Prospector AB We present the first in situ measurements of the secondary electron emission efficiency of lunar regolith, utilizing Lunar Prospector measurements of secondary electrons emitted from the negatively charged night side and accelerated upward by surface electric fields. By comparing measurements of secondary currents emitted from the surface and incident primary electron currents, we find that the secondary yield of lunar regolith is a factor of similar to 3 lower than that measured for samples in the laboratory. This lower yield significantly affects current balance at the lunar surface and the resulting equilibrium surface potentials. This information must be folded into models of the near-surface plasma sheath, in order to predict the effects on dust and other components of the lunar environment, and ultimately determine the importance for surface exploration and scientific investigations on the Moon. (C) 2008 Elsevier Ltd. All rights reserved. C1 [Halekas, J. S.; Delory, G. T.; Lin, R. P.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Lin, R. P.] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA. [Stubbs, T. J.] Univ Maryland Baltimore Cty, Goddard Earth Sci & Technol Ctr, Baltimore, MD 21228 USA. [Stubbs, T. J.; Farrell, W. M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Halekas, JS (reprint author), Univ Calif Berkeley, Space Sci Lab, 7 Gauss Way, Berkeley, CA 94720 USA. EM jazzman@ssi.berkeley.edu RI Stubbs, Timothy/I-5139-2013; Farrell, William/I-4865-2013; OI Stubbs, Timothy/0000-0002-5524-645X; Halekas, Jasper/0000-0001-5258-6128 FU NASA [NNG06GJ23G, NNX07AG10G] FX This work was supported by the NASA grants NNG06GJ23G and NNX07AG10G. NR 10 TC 25 Z9 26 U1 0 U2 3 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 JAN PY 2009 VL 57 IS 1 BP 78 EP 82 DI 10.1016/j.pss.2008.11.009 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 409OK UT WOS:000263515300010 ER PT B AU Khazanov, GV Tel'nikhin, AA Kronberg, TK AF Khazanov, G. V. Tel'nikhin, A. A. Kronberg, T. K. BE Gromov, SP TI CHAOTIC MOTION OF RELATIVISTIC ELECTRONS DRIVEN BY WHISTLER WAVES SO PLASMA PHYSICS RESEARCH ADVANCES LA English DT Article; Book Chapter ID JOVIAN MAGNETOSPHERE; PARTICLE; ACCELERATION; DIFFUSION; JUPITER; PACKET; FIELD AB Canonical equations governing all electron motion in electromagnetic field of the whistler mode waves propagating along the direction of an ambient magnetic field are derived. The physical processes on which the equations of motion are based are identified. It is shown that relativistic electrons interacting with these fields demonstrate chaotic motion, which is accompanied by the particle stochastic heating and significant pitch angle diffusion. Evolution of distribution functions is described by the Fokker-Planck-Kolmogorov equations. A coefficient of diffusion is calculated from the equations of motion. Our results indicate that phase flow Of Our dynamical system is structural stable strange attractor. Chaotic motion on the attractor gives rise to an irreversible process (the so-called deterministic diffusion), which leads actually to establishing a steady-state energy spectra and results in such important and easily observable effects as the stochastic heating and pitch angle scattering of plasma particles. Under conditions typical of this mechanism, the heating region is determined by the boundaries of the attractor, and the heating rate is governed by the nature of the kinetics, which in turn depends on the canonical variables on the attractor. The same conditions impose limitations on the timescales of macroscopic effects and feasible extent of heating, so that understanding of this condition is of great practical interest. It is shown that the whistler mode waves could provide a viable mechanism for stochastic energization of electrons with energies up to 50 MeV in the Jovian magnetosphere. C1 [Khazanov, G. V.] NASA Marshall Space Flight Ctr, Natl Space Sci & Technol Ctr, Huntsville, AL 35805 USA. [Tel'nikhin, A. A.; Kronberg, T. K.] Altai State Univ, Barnaul 656049, Russia. RP Khazanov, GV (reprint author), NASA Marshall Space Flight Ctr, Natl Space Sci & Technol Ctr, 320 Sparkman Dr, Huntsville, AL 35805 USA. NR 27 TC 0 Z9 0 U1 0 U2 0 PU NOVA SCIENCE PUBLISHERS, INC PI HAUPPAUGE PA 400 OSER AVE, STE 1600, HAUPPAUGE, NY 11788-3635 USA BN 978-1-60456-136-4 PY 2009 BP 333 EP 355 PG 23 WC Chemistry, Physical; Physics, Fluids & Plasmas SC Chemistry; Physics GA BKX66 UT WOS:000269533400010 ER PT S AU Quijada, MA Waluschka, E Wilson, M McClain, CR AF Quijada, Manuel A. Waluschka, Eugene Wilson, Mark McClain, Charles R. BE Shaw, JA Tyo, JS TI Measured Performance for Proposed Depolarizer for the Ocean Radiometer for Carbon Assessment SO POLARIZATION SCIENCE AND REMOTE SENSING IV SE Proceedings of SPIE LA English DT Proceedings Paper CT Conference on Polarization Science and Remote Sensing IV CY AUG 03-04, 2009 CL San Diego, CA SP SPIE DE ORCA; Polarimetry; depolarizer; birefringent materials; Mueller matrices AB The Ocean Radiometer for Carbon Assessment (ORCA) is a new design concept for the next generation ocean biology and biogeochemistry satellite sensor. The wavelength range will be from the near UV, through the visible and to the Short Wave infrared. The challenge in this design is to remove the polarization effects from the optical performance of this hyper spectral observing instrument. In order to remove any polarization sensitivity during observation, the design calls for a front-end depolarizer that consists of two wedged birefringent magnesium fluoride crystals. Here we discuss the polarimetry measurements performed on this polarization scrambler, the depolarizer design and compare these results with model calculations. C1 [Quijada, Manuel A.; Waluschka, Eugene; Wilson, Mark; McClain, Charles R.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Quijada, MA (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. EM manuel.a.quijada@nasa.gov NR 6 TC 1 Z9 1 U1 0 U2 1 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 978-0-8194-7751-4 J9 PROC SPIE PY 2009 VL 7461 AR 746105 DI 10.1117/12.827427 PG 10 WC Remote Sensing; Optics SC Remote Sensing; Optics GA BCJ99 UT WOS:000310357000004 ER PT S AU Westl, E Gary, GA Cirtain, J Davis, J Kobayashi, K Pietraszewski, C AF Westl, Edward Gary, G. Allen Cirtain, Jonathan Davis, John Kobayashi, Ken Pietraszewski, Chris BE Shaw, JA Tyo, JS TI CIV Polarization Measurements using a Vacuum Ultraviolet Fabry-Perot Interferometer SO POLARIZATION SCIENCE AND REMOTE SENSING IV SE Proceedings of SPIE LA English DT Proceedings Paper CT Conference on Polarization Science and Remote Sensing IV CY AUG 03-04, 2009 CL San Diego, CA SP SPIE DE Fabry-Perot Interferometer; VUV Fabry-Perot; Vacuum Ultraviolet; Polarization; CIV measurement ID REGION AB Marshall Space Flight Center's (MSFC) is developing a Vacuum Ultraviolet (VUV) Fabry-Perot Interferometer that will be launched on a sounding rocket for high throughput, high-cadence, extended field of view CIV (155nm) measurements. These measurements will provide (i) Dopplergrams for studies of waves, oscillations, explosive events, and mass motions through the transition region, and, (ii), polarization measurements to study the magnetic field in the transition region. This paper will describe the scientific goals of the instrument, a brief description of the optics and the polarization characteristics of the VUV Fabry Perot. C1 [Westl, Edward; Cirtain, Jonathan; Davis, John] NASA, George C Marshall Space Flight Ctr, Space Sci Off, VP62, Huntsville, AL 35812 USA. [Gary, G. Allen; Kobayashi, Ken] Univ Alabama, CSPAR, Huntsville, AL 35899 USA. [Pietraszewski, Chris] IC Opt Syst Ltd, Berkshire, England. RP Westl, E (reprint author), NASA, George C Marshall Space Flight Ctr, Space Sci Off, VP62, Huntsville, AL 35812 USA. NR 17 TC 0 Z9 0 U1 0 U2 1 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 978-0-8194-7751-4 J9 PROC SPIE PY 2009 VL 7461 AR UNSP 746103 DI 10.1117/12.825718 PG 11 WC Remote Sensing; Optics SC Remote Sensing; Optics GA BCJ99 UT WOS:000310357000002 ER PT J AU Smith, TM Williams, MK Fesmire, JE Sass, JP Weiser, ES AF Smith, Trent M. Williams, Martha K. Fesmire, James E. Sass, Jared P. Weiser, Erik S. BE Mittal, KL TI Polyimide-Aerogel Hybrid Foam Composites for Advanced Applications SO POLYIMIDES AND OTHER HIGH-TEMPERATURE POLYMERS: SYNTHESIS, CHARACTERIZATION AND APPLICATIONS, VOL 5 LA English DT Proceedings Paper CT 5th International Symposium on Polyimides and Other High-Temperature Polymers - Synthesis, Characterization and Applications/MST Conferences CY NOV 05-07, 2007 CL Orlando, FL SP MST Conf DE Polyimide; aerogel; foam; foam composite; aerospace insulation; high-performance foam; TEEK ID POLYURETHANE-BASED AEROGELS; COHERENT EXPANDED AEROGELS; LINKED SILICA AEROGELS; THERMAL-RESISTANCE; INSULATION; PERFORMANCE; PRECURSORS; DENSITY AB NASA has had a growing need for high-performance polymer foams for cryogenic insulation, fireproofing, energy absorption and other applications. Commercially available foams, however, do not meet all of the requirements for surviving extreme environments. Most low-density foams crack at cryogenic temperatures, and the foams that can withstand extreme temperatures do not have the required structural integrity or thermal performance. Chemists and Engineers at NASA's Kennedy Space Center and Langley Research Center have collaborated in the development of a polyimide foam composite based on TEEK polyimide foam technology with enhanced thermal performance and vibration attenuation properties. The foam composites can be fabricated to target densities: high-density foam composites for structural applications and low-density foam composites where more flexibility might be advantageous. Heat transfer reduction is driven primarily by inorganic aerogel filler, with aerogel blanket composites having the most significant reduction in heat transfer and vibration attenuation. The TEEK composites are fire resistant and have excellent weather-resistant properties. This composite technology also lends itself to other foam systems. These materials may prove useful in process fluid piping, tanks for transporting and storing hot or cold fluids, ship and boat building and especially aerospace applications. C1 [Smith, Trent M.; Williams, Martha K.; Fesmire, James E.; Sass, Jared P.] NASA, John F Kennedy Space Ctr, Spaceport Technol Div, Kennedy Space Ctr, FL 32899 USA. RP Smith, TM (reprint author), NASA, John F Kennedy Space Ctr, Spaceport Technol Div, Kennedy Space Ctr, FL 32899 USA. EM Trent.M.Smith@nasa.gov NR 31 TC 0 Z9 0 U1 3 U2 26 PU E J BRILL PI PA LEIDEN PA PO BOX 9000, NL-2300 PA LEIDEN, NETHERLANDS BN 978-90-474-2411-6 PY 2009 BP 295 EP 305 PG 11 WC Polymer Science SC Polymer Science GA BBY83 UT WOS:000308911600017 ER PT S AU Baran, O DeGennaro, A Rame, E Wilkinson, A AF Baran, Oleh DeGennaro, Alfred Rame, Enrique Wilkinson, Allen BE Nakagawa, M Luding, S TI DEM Simulation of a Schulze Ring Shear Tester SO POWDERS AND GRAINS 2009 SE AIP Conference Proceedings LA English DT Proceedings Paper CT 6th International Conference on the Micromechanics of Granular Media CY JUL 13-17, 2009 CL Golden, CO SP Assoc Study Micromech Granular Media, Univ Twente, Colorado Sch Mines DE DEM; EDEM; granular flow; Schulze ring shear test AB The Schulze ring shear tester allows measurement of yield loci for bulk granular solids and of the friction between the solids and the container wall material. These measurements are required inputs in a systematic design method for hoppers. The measurements are subject to test-to-test variations caused by the combined effects of several factors, such as cell filling technique, sampling technique, particle size and shape distribution of the loaded sample and cell size relative to the particle size. One difficulty for the experimenter is to decide which factors are most important in the shear test outcome. In this paper, we validate Discrete Element Model (DEM) simulation parameters with physical measurements of the JSC-1A lunar soil simulant, and inform about the relative impact of the various parameters to the shear test outcome. Specific tests will include sensitivity studies using DEM simulations that probe the effects of particle-to-cell size ratio, particle size distribution, particle shape, shear modulus and inter-particle adhesion and friction on shear failure. C1 [Baran, Oleh] DEM Solut Inc, Lebanon, NH USA. [DeGennaro, Alfred; Rame, Enrique; Wilkinson, Allen] NASA, Glenn Res Ctr, Cleveland, OH USA. RP Baran, O (reprint author), DEM Solut Inc, Lebanon, NH USA. NR 10 TC 0 Z9 0 U1 2 U2 6 PU AMER INST PHYSICS PI MELVILLE PA 2 HUNTINGTON QUADRANGLE, STE 1NO1, MELVILLE, NY 11747-4501 USA SN 0094-243X BN 978-0-7354-0682-7 J9 AIP CONF PROC PY 2009 VL 1145 BP 409 EP + PG 2 WC Materials Science, Multidisciplinary; Mechanics SC Materials Science; Mechanics GA BLN80 UT WOS:000270602900091 ER PT S AU Metzger, PT Latta, RC Schuler, JA Immer, CD AF Metzger, Philip T. Latta, Robert C., III Schuler, Jason A. Immer, Christopher D. BE Nakagawa, M Luding, S TI Craters Formed in Granular Beds by Impinging Jets of Gas SO POWDERS AND GRAINS 2009 SE AIP Conference Proceedings LA English DT Proceedings Paper CT 6th International Conference on the Micromechanics of Granular Media CY JUL 13-17, 2009 CL Golden, CO SP Assoc Study Micromech Granular Media, Univ Twente, Colorado Sch Mines DE crater; erosion; scour hole; jet; bearing capacity; rocket exhaust; martian soil; gravity ID EROSION AB When a jet of gas impinges vertically on a granular bed and forms a crater, the grains may be moved by several different mechanisms: viscous erosion, diffused gas eruption, bearing capacity failure, and/or diffusion-driven shearing. The relative importance of these mechanisms depends upon the flow regime of the gas, the mechanical state of the granular material, and other physical parameters. Here we report research in two specific regimes: viscous erosion forming scour holes as a function of particle size and gravity; and bearing capacity failure forming deep transient craters as a function of soil compaction. C1 [Metzger, Philip T.] NASA, Granular Mech & Regolith Operat Lab, Kennedy Space Ctr, FL 32899 USA. RP Metzger, PT (reprint author), NASA, Granular Mech & Regolith Operat Lab, Kennedy Space Ctr, FL 32899 USA. OI Metzger, Philip/0000-0002-6871-5358 NR 8 TC 6 Z9 6 U1 0 U2 0 PU AMER INST PHYSICS PI MELVILLE PA 2 HUNTINGTON QUADRANGLE, STE 1NO1, MELVILLE, NY 11747-4501 USA SN 0094-243X BN 978-0-7354-0682-7 J9 AIP CONF PROC PY 2009 VL 1145 BP 767 EP 770 PG 4 WC Materials Science, Multidisciplinary; Mechanics SC Materials Science; Mechanics GA BLN80 UT WOS:000270602900174 ER PT B AU Ryan, S AF Ryan, Shannon BE Hiermaier, S TI Numerical Simulation in Micrometeoroid and Orbital Debris Risk Assessment SO PREDICTIVE MODELING OF DYNAMIC PROCESSES: A TRIBUTE TO PROFESSOR KLAUS THOMA LA English DT Article; Book Chapter ID BALLISTIC LIMIT; HYPERVELOCITY; SPACECRAFT; IMPACT; VELOCITIES AB The threat of micrometeoroid and orbital debris (MMOD) impacts on space vehicles is assessed in terms of the probability of an impactor penetrating the spacecraft hull, and the probability of a penetrating impact resulting in catastrophic failure. These values are calculated in risk analysis codes which combine spacecraft geometry, debris environment models, and equations that define the penetration limits of the spacecraft outer structure (called ballistic limit equations, or BLEs). To characterize the performance of spacecraft structures under impact of MMOD particles at hypervelocity, experimental facilities such as two-stage light gas guns are commonly used. However, these facilities are only capable of reproducing approximately 40% of expected in-orbit impact conditions. As a result, numerical techniques are ideally suited for application in this field. The use of numerical hydrocodes in MMOD risk assessment is, historically, very limited. However, as code maturity continues to develop, their application becomes increasingly accepted. Within this chapter three examples are presented in which numerical hydrocodes were used in tandem with experimental testing for MMOD risk assessments. Beginning with the most simplistic application, i.e. derivation of perforation limits, the examples extend to the propagation of impact-induced dynamic disturbances through complex satellite structures. C1 NASA, Johnson Space Ctr, Lunar & Planetary Inst, USRA, Washington, DC 20546 USA. RP Ryan, S (reprint author), NASA, Johnson Space Ctr, Lunar & Planetary Inst, USRA, Washington, DC 20546 USA. EM Shan-non.j.ryan@nasa.gov NR 27 TC 2 Z9 2 U1 0 U2 0 PU SPRINGER PI NEW YORK PA 233 SPRING STREET, NEW YORK, NY 10013, UNITED STATES BN 978-1-4419-0726-4 PY 2009 BP 417 EP 446 DI 10.1007/978-1-4419-0727-1_22 D2 10.1007/978-1-4419-0727-1 PG 30 WC Engineering, Multidisciplinary; Engineering, Mechanical; Transportation Science & Technology SC Engineering; Transportation GA BLA90 UT WOS:000269796700023 ER PT S AU Vetere, L Burrows, DN Gehrels, N Meszaros, P Wang, X AF Vetere, L. Burrows, D. N. Gehrels, N. Meszaros, P. Wang, X. BE Antonelli, LA Limongi, M Menci, N Tornambe, A Brocato, E Raimondo, G TI GRBs with no afterglow even in the Swift Era? SO PROBING STELLAR POPULATIONS OUT TO THE DISTANT UNIVERSE SE AIP Conference Proceedings LA English DT Proceedings Paper CT International Conference on Probing Stellar Populations Out to the Distant Universe CY SEP 07-19, 2008 CL Cefalu, ITALY SP Italian Inst Astrophys, Italian Inst Astrophys, Astron Observ Rome, Italian Inst Astrophys, Astron Observ Palermo, Italian Inst Astrophys, Astron Observ Teramo, Univ Cagliari, Dept Phys, Univ Palermo, Dept Phys & Astron Sci, Cefalu Local Author, Mondralisco Fdn, Assoc Cefalu & Astron DE X-ray; gamma-ray; gamma-ray bursts AB Thanks to its great capability Swift succeeds detecting an afterglow more than 93% of the time BAT triggers a new event. In a few cases, mainly Short GRBs or late observations, XRT did not detect any emission. However, for at least seven Long GRBs XRT could not measure any X-afterglow either, even as early as 100s after the BAT trigger. The detection of this new class of GRBs without any X-ray emission has raised many questions. Are these extreme naked GRB? Is this a completely new class of objects with an uncommon emission release? In this contribution we present a study on these unusual events. We analyse their peculiar behaviour in the Gamma and X-ray bands and discuss their singular origin. C1 [Vetere, L.; Burrows, D. N.; Meszaros, P.] Penn State Univ, Dept Astron & Astrophys, 525 Davey Lab, University Pk, PA 16802 USA. [Gehrels, N.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Wang, X.] Nanjing Univ, Dept Astron, Nanjing 210093, Peoples R China. RP Vetere, L (reprint author), Penn State Univ, Dept Astron & Astrophys, 525 Davey Lab, University Pk, PA 16802 USA. EM vetere@astro.psu.edu RI Gehrels, Neil/D-2971-2012 NR 3 TC 0 Z9 0 U1 0 U2 0 PU AMER INST PHYSICS PI MELVILLE PA 2 HUNTINGTON QUADRANGLE, STE 1NO1, MELVILLE, NY 11747-4501 USA SN 0094-243X BN 978-0-7354-0648-3 J9 AIP CONF PROC PY 2009 VL 1111 BP 370 EP + PG 2 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BJK00 UT WOS:000266597500061 ER PT S AU De Pasquale, M Evans, P Oates, S Page, M Zane, S Breeveld, A Holland, S Still, A AF De Pasquale, M. Evans, P. Oates, S. Page, M. Zane, S. Breeveld, A. Holland, S. Still, A. BE Antonelli, LA Limongi, M Menci, N Tornambe, A Brocato, E Raimondo, G TI Jet breaks at the end of the plateau phase of Swift GRB lightcurves SO PROBING STELLAR POPULATIONS OUT TO THE DISTANT UNIVERSE SE AIP Conference Proceedings LA English DT Proceedings Paper CT International Conference on Probing Stellar Populations Out to the Distant Universe CY SEP 07-19, 2008 CL Cefalu, ITALY SP Italian Inst Astrophys, Italian Inst Astrophys, Astron Observ Rome, Italian Inst Astrophys, Astron Observ Palermo, Italian Inst Astrophys, Astron Observ Teramo, Univ Cagliari, Dept Phys, Univ Palermo, Dept Phys & Astron Sci, Cefalu Local Author, Mondralisco Fdn, Assoc Cefalu & Astron DE high energy astrophysics; relativistic outflows AB An increasing sample of Swift GRBs show evidence of 'chromatic breaks', i.e. breaks that are present in the X-ray but not in the optical. Modelling the X-ray and optical data, we find that in a significant fraction of these GRB afterglows the component producing the X-ray emission cannot be responsible for the optical emission too. We propose that these afterglow lightcurves are the result of a two-component jet, in which both components are energy-injected for the whole observation and the X-ray break is due to a jet break in the narrow outflow. Bursts with chromatic breaks provide us with an explanation for another surprising finding, the paucity of late achromatic breaks. We show that our model may explain the behaviour of GRB emission in both X-ray and optical bands. Therefore, it can be a radical and noteworthy alternative to the current interpretation for the 'canonical' XRT and UVOT lightcurves, bearing fundamental implications for GRB physics. C1 [De Pasquale, M.; Oates, S.; Page, M.; Zane, S.; Breeveld, A.; Still, A.] Univ Coll London, Mullard Space Lab, Holmbury Rd, Dorking RH5 6NT, Surrey, England. [Evans, P.] Univ Leicester, Leicester LE1 7RH, Leics, England. [Holland, S.] Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP De Pasquale, M (reprint author), Univ Coll London, Mullard Space Lab, Holmbury Rd, Dorking RH5 6NT, Surrey, England. EM mpd@mssl.ucl.ac.uk FU Royal Astronomical Society FX The author could attend the Cefalu' conference and give his talk thanks to a grant from Royal Astronomical Society. NR 5 TC 0 Z9 0 U1 0 U2 2 PU AMER INST PHYSICS PI MELVILLE PA 2 HUNTINGTON QUADRANGLE, STE 1NO1, MELVILLE, NY 11747-4501 USA SN 0094-243X BN 978-0-7354-0648-3 J9 AIP CONF PROC PY 2009 VL 1111 BP 379 EP + PG 2 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BJK00 UT WOS:000266597500063 ER PT B AU Boyle, RJ Jones, SM AF Boyle, R. J. Jones, S. M. GP ASME TI Effects of Precooling Turbine Cooling Air on Engine Performance SO PROCEEDINGS OF ASME TURBO EXPO 2009, VOL 4 LA English DT Proceedings Paper CT 54th ASME Turbo Expo 2009 CY JUN 08-12, 2009 CL Orlando, FL SP ASME, Int Gas Turbine Inst AB Approaches to improving gas turbine cycle efficiency by cooling the compressor discharge air used for turbine cooling are explored. From a turbine cycle standpoint, cooling the coolant air can improve cycle efficiency. A significant improvement in specific fuel consumption is achieved by raising the turbine rotor inlet temperature, and engine pressure ratio. Precooling compressor discharge air can enable rotor inlet temperature to increase up to 100 K at the same rotor cooling flow rate ratio. The efficiency gains from a 100 K rise in rotor inlet temperature translated into a fuel savings of 400 kg for a mission length of 5450 km. This fuel savings means about a 1200 kg savings in CO2 production. Compressor discharge air that passes through a heat exchanger may not have enough pressure to prevent hot gas ingestion through the cooling holes of the high pressure turbine stator. A stator analysis assuming a mixture of precooled and uncooled compressor discharge air showed only a 50 K rise in rotor inlet temperature due to precooling at the same cooling flow rate ratio. C1 [Boyle, R. J.; Jones, S. M.] NASA, Glenn Res Ctr, Cleveland, OH USA. RP Boyle, RJ (reprint author), NASA, Glenn Res Ctr, Cleveland, OH USA. EM Robert.J.Boyle@nasa.gov; Scott.M.Jones@nasa.gov NR 16 TC 0 Z9 0 U1 0 U2 1 PU AMER SOC MECHANICAL ENGINEERS PI NEW YORK PA THREE PARK AVENUE, NEW YORK, NY 10016-5990 USA BN 978-0-7918-4885-2 PY 2009 BP 495 EP 504 PG 10 WC Engineering, Mechanical; Materials Science, Multidisciplinary; Metallurgy & Metallurgical Engineering SC Engineering; Materials Science; Metallurgy & Metallurgical Engineering GA BON26 UT WOS:000277058700046 ER PT B AU Bruckner, RJ AF Bruckner, Robert J. GP ASME TI WINDAGE POWER LOSS IN GAS FOIL BEARINGS AND THE ROTOR-STATOR CLEARANCE OF HIGH SPEED GENERATORS OPERATING IN HIGH PRESSURE ENVIRONMENTS SO PROCEEDINGS OF ASME TURBO EXPO 2009, VOL 5 LA English DT Proceedings Paper CT 54th ASME Turbo Expo 2009 CY JUN 08-12, 2009 CL Orlando, FL SP ASME, Int Gas Turbine Inst AB Closed Brayton Cycle (CBC) and Closed Supercritical Cycle (CSC) engines are prime candidates to convert heat from a reactor into electric power for robotic space exploration and habitation. These engine concepts incorporate a permanent magnet starter / generator mounted on the engine shaft along with the requisite turbomachinery. Successful completion of the long duration missions currently anticipated for these engines will require designs that adequately address all losses within the machine. The preliminary thermal management concept for these engine types is to use the cycle working fluid to provide the required cooling. In addition to providing cooling, the working fluid will also serve as the bearing lubricant. Additional requirements due to the unique application of these microturbines are zero contamination of the working fluid and entirely maintenance-free operation for many years. Losses in the gas foil bearings and within the rotor-stator gap of the generator become increasingly important as both rotational speed and mean operating pressure are increased. This paper presents the results of an experimental study, which obtained direct torque measurements on gas foil bearings and generator rotor-stator gaps. Test conditions for these measurements included rotational speeds up to 42000 revolutions per minute, pressures up to 45 atmospheres, and test gases of Nitrogen, Helium, and Carbon Dioxide. These conditions provided a maximum test Taylor number of nearly one million. The results show an exponential rise in power loss as mean operating density is increased for both the gas foil bearing and generator windage. These typical "secondary" losses can become larger than the total system output power if conventional design paradigms are followed. A non-dimensional analysis is presented to extend the experimental results into the CSC range for the generator windage. C1 NASA, Glenn Res Ctr, Cleveland, OH USA. RP Bruckner, RJ (reprint author), NASA, Glenn Res Ctr, Cleveland, OH USA. NR 22 TC 1 Z9 2 U1 0 U2 1 PU AMER SOC MECHANICAL ENGINEERS PI NEW YORK PA THREE PARK AVENUE, NEW YORK, NY 10016-5990 USA BN 978-0-7918-4886-9 PY 2009 BP 263 EP 270 PG 8 WC Energy & Fuels; Engineering, Mechanical SC Energy & Fuels; Engineering GA BON28 UT WOS:000277059700027 ER PT S AU Eberspeaker, PJ Gregory, DD AF Eberspeaker, P. J. Gregory, D. D. BE Lacoste, H TI AN OVERVIEW OF THE NASA SOUNDING ROCKETS AND BALLOON PROGRAMS SO PROCEEDINGS OF THE 19TH ESA SYMPOSIUM ON EUROPEAN ROCKET AND BALLOON PROGRAMMES AND RELATED RESEARCH SE ESA Special Publications LA English DT Proceedings Paper CT 19th ESA Symposium on European Rocket and Balloon Programmes and Related Research CY JUN 07-11, 2009 CL Bad Reichenhall, GERMANY SP European Space Agcy (ESA) AB The U. S. National Aeronautics and Space Administration (NASA) Sounding Rockets and Balloon Programs conduct a combined total of 40 to 50 missions per year in support of the NASA scientific community and other users. The NASA Sounding Rockets Program supports the science community by integrating their experiments into the sounding rocket payloads, and providing both the rocket vehicle and launch operations services. Flight operations have been conducted at Andoya Rocket Range, Poker Flat Research Range, Whites Sands Missile Range and Wallops Flight Facility. Development efforts include the Mesquito and Terrier-Improved Malemute launch vehicles as well as new attitude sensors and systems. The NASA Balloon Program provides balloons, data acquisition, and launch and flight operations support to the science community. Flight operations have been conducted in Antarctica; Sweden (Esrange); Palestine, Texas; and Ft. Sumner, New Mexico. Flights have included conventional and long duration balloons as well as a successful demonstration flight of the NASA Super Pressure Balloon. Technology initiatives include the development of parachute shock attenuation systems and an upgraded gondola automatic parachute release system. C1 [Eberspeaker, P. J.] NASA, Sounding Rocket Program Off, Goddard Space Flight Ctr, Wallops Flight Facil, Wallops Isl, VA 23337 USA. RP Eberspeaker, PJ (reprint author), NASA, Sounding Rocket Program Off, Goddard Space Flight Ctr, Wallops Flight Facil, Wallops Isl, VA 23337 USA. EM philip.j.eberspeaker@nasa.gov NR 4 TC 0 Z9 0 U1 0 U2 0 PU EUROPEAN SPACE AGENCY PI PARIS PA 8-10 RUE MARIO NIKIS, 75738 PARIS, FRANCE SN 0379-6566 BN 978-92-9221-235-3 J9 ESA SPEC PUBL PY 2009 VL 671 BP 27 EP 34 PG 8 WC Engineering, Aerospace; Astronomy & Astrophysics; Meteorology & Atmospheric Sciences SC Engineering; Astronomy & Astrophysics; Meteorology & Atmospheric Sciences GA BBY59 UT WOS:000308797400006 ER PT B AU Aranki, N Keymeulen, D Bakhshi, A Klimesh, M AF Aranki, Nazeeh Keymeulen, Didier Bakhshi, Alireza Klimesh, Matthew GP IEEE/Computer Soc TI Hardware Implementation of Lossless Adaptive and Scalable Hyperspectral Data Compression for Space SO PROCEEDINGS OF THE 2009 NASA/ESA CONFERENCE ON ADAPTIVE HARDWARE AND SYSTEMS LA English DT Proceedings Paper CT 4th NASA/ESA Conference on Adaptive Hardware and Systems CY JUL 29-AUG 01, 2009 CL Moscone Convention Ctr, San Francisco, CA SP NASA Jet Propuls Lab, European Space Agcy, Univ Edinburgh HO Moscone Convention Ctr AB On-board lossless hyperspectral data compression reduces data volume in order to meet NASA and DoD limited downlink capabilities. The technique also improves signature extraction, object recognition and feature classification capabilities by providing exact reconstructed data on constrained downlink resources. At JPL a novel, adaptive and predictive technique for lossless compression of hyperspectral data was recently developed This technique uses an adaptive filtering method and achieves a combination of low complexity and compression effectiveness that far exceeds state-of-the-art techniques currently in use. The JPL-developed 'Fast Lossless' algorithm requires no training data or other specific information about the nature of the spectral bands for a fixed instrument dynamic range. It is of low computational complexity and thus well-suited for implementation in hardware. A modified form of the algorithm that is better suited for data from pushbroom instruments is generally appropriate for flight implementation. A scalable field programmable gate array (FPGA) hardware implementation was developed The FPGA implementation achieves a throughput performance of 58 Msamples/sec, which can be increased to over 100 Msamples/sec in a parallel implementation that uses twice the hardware resources This paper describes the hardware implementation of the 'Modified Fast Lossless' compression algorithm on an FPGA. The FPGA implementation targets the current state-of-the-art FPGAs (Xilinx Virtex IV and V families) and compresses one sample every clock cycle to provide a fast and practical real-time solution for space applications. C1 [Aranki, Nazeeh; Keymeulen, Didier; Klimesh, Matthew] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. [Bakhshi, Alireza] B&A Engn Inc, San Dimas, CA 91773 USA. RP Aranki, N (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM nazeeh.aranki@jpl.nasa.gov FU Jet Propulsion Laboratory; California Institute of Technology; National Aeronautics and Space Administration; Air Force Research Laboratory; JPL FX The work 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. This work was funded by Air Force Research Laboratory through the grant entitled Fast Lossless On-Board Hyperspectral Data Compression. Special thanks to Randy Odle, program manager, who also supported this research at JPL, and to Ian Ferguson for his technical support to this research NR 24 TC 6 Z9 6 U1 0 U2 5 PU IEEE COMPUTER SOC PI LOS ALAMITOS PA 10662 LOS VAQUEROS CIRCLE, PO BOX 3014, LOS ALAMITOS, CA 90720-1264 USA BN 978-0-7695-3714-6 PY 2009 BP 315 EP + DI 10.1109/AHS.2009.66 PG 2 WC Computer Science, Theory & Methods; Engineering, Electrical & Electronic SC Computer Science; Engineering GA BVA38 UT WOS:000290894400041 ER PT B AU Kizhner, S Heinzen, K AF Kizhner, Semion Heinzen, Katherine GP IEEE/Computer Soc TI New Methodology for Reducing Sensor and Readout Electronics Circuitry Noise in Digital Domain SO PROCEEDINGS OF THE 2009 NASA/ESA CONFERENCE ON ADAPTIVE HARDWARE AND SYSTEMS LA English DT Proceedings Paper CT 4th NASA/ESA Conference on Adaptive Hardware and Systems CY JUL 29-AUG 01, 2009 CL Moscone Convention Ctr, San Francisco, CA SP NASA Jet Propuls Lab, European Space Agcy, Univ Edinburgh HO Moscone Convention Ctr AB Upcoming NASA cosmology survey missions, such as Joint Dark Energy Mission (JDEM), carry instruments with multiple focal planes populated with many large sensor detector arrays. These sensors are passively cooled to low temperatures for low-level light and near-infrared (NIR) signal detection, and the sensor readout electronics circuitry must perform at extremely low noise levels to enable new required science measurements. Because we are at the technological edge of enhanced performance for sensors and readout electronics circuitry, as determined by thermal noise level at given temperature in analog domain, we must find new ways of further compensating for the noise in the signal digital domain. To facilitate this new approach, state-of-the-art sensors are augmented at their array hardware boundaries by non-illuminated or non-sensitive to photons reference pixels, which can be used to reduce noise attributed to sensor and readout electronics. There are a few proposed methodologies of processing in the digital domain the information carried by reference pixels. These methods involve using spatial and temporal global statistical scalar parameters derived from boundary reference pixel information to enhance the active pixels' signals. To make a step beyond this heritage methodology, we apply the NASA-developed technology known as the Hilbert-Huang Transform Data Processing System (HHT-DPS) to some component of reference pixel vectors' information. This allows to derive a noise correction array, which, in addition to the statistical parameter over the signal trend, is applied to the active pixel array. C1 [Kizhner, Semion; Heinzen, Katherine] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Kizhner, S (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt Rd, Greenbelt, MD 20771 USA. EM Semion.Kizhner-1@nasa.gov NR 8 TC 0 Z9 0 U1 0 U2 4 PU IEEE COMPUTER SOC PI LOS ALAMITOS PA 10662 LOS VAQUEROS CIRCLE, PO BOX 3014, LOS ALAMITOS, CA 90720-1264 USA BN 978-0-7695-3714-6 PY 2009 BP 323 EP 329 DI 10.1109/AHS.2009.15 PG 7 WC Computer Science, Theory & Methods; Engineering, Electrical & Electronic SC Computer Science; Engineering GA BVA38 UT WOS:000290894400042 ER PT J AU Esterhuizen, S Franklin, G Hurst, K Mannucci, A Meehan, T Webb, F Young, L AF Esterhuizen, Stephan Franklin, Garth Hurst, Ken Mannucci, Anthony Meehan, Tom Webb, Frank Young, Larry BA Wang, J Feng, Y Wang, C BF Wang, J Feng, Y Wang, C TI TriG - A GNSS Precise Orbit and Radio Occultation Space Receiver SO PROCEEDINGS OF THE 22ND INTERNATIONAL TECHNICAL MEETING OF THE SATELLITE DIVISION OF THE INSTITUTE OF NAVIGATION (ION GNSS 2009) LA English DT Proceedings Paper CT 22nd International Technical Meeting of the Satellite Division of the Institute-of-Navigation (ION GNSS-09) CY SEP 22-25, 2009 CL Savannah, GA AB The GPS radio occultation (RO) technique [1] produces measurements in the ionosphere and neutral atmosphere [2] that contribute to monitoring space weather and climate change; and improving operational weather prediction. The high accuracy of RO soundings, traceable to SI standards, makes them ideal climate benchmark observations. For weather applications, RO observations improve the accuracy of weather forecasts by providing temperature and moisture profiles of sub-km vertical resolution, over land and ocean and in the presence of clouds. JPL is currently flying a handful of RO instruments [3] on various satellites in Low Earth Orbit (LEO). Although these receivers have served to pioneer occultation measurements, various advances in technology and understanding of the RO technique along with availability of new signals from GPS and other GNSS satellites allow us to design an improved next generation space-based Precise Orbit Determination (POD) and RO receiver, the TriG receiver. The paper describes the architecture and implementation of the JPL TriG receiver as well as results obtained with a prototype receiver demonstrating key technologies necessary for a next-generation space science receiver. C1 [Esterhuizen, Stephan; Franklin, Garth; Hurst, Ken; Mannucci, Anthony; Meehan, Tom; Webb, Frank; Young, Larry] CALTECH, JPL, Pasadena, CA 91125 USA. RP Esterhuizen, S (reprint author), CALTECH, JPL, Pasadena, CA 91125 USA. NR 6 TC 3 Z9 3 U1 0 U2 0 PU INST NAVIGATION PI WASHINGTON PA 815 15TH ST NW, STE 832, WASHINGTON, DC 20005 USA PY 2009 BP 1442 EP 1446 PG 5 WC Computer Science, Artificial Intelligence; Telecommunications SC Computer Science; Telecommunications GA BSG19 UT WOS:000284356201048 ER PT S AU Roychoudhury, I Biswas, G Koutsoukos, X AF Roychoudhury, Indranil Biswas, Gautam Koutsoukos, Xenofon GP IEEE TI Factoring Dynamic Bayesian Networks Based on Structural Observability SO PROCEEDINGS OF THE 48TH IEEE CONFERENCE ON DECISION AND CONTROL, 2009 HELD JOINTLY WITH THE 2009 28TH CHINESE CONTROL CONFERENCE (CDC/CCC 2009) SE IEEE Conference on Decision and Control LA English DT Proceedings Paper CT Joint 48th IEEE Conference on Decision and Control (CDC) / 28th Chinese Control Conference (CCC) CY DEC 15-18, 2009 CL Shanghai, PEOPLES R CHINA SP IEEE, Honeywell, Quanser, United Technologies, Googol Tech, MathWorks, Natl Instruments ID LINEAR-SYSTEMS AB Dynamic Bayesian Networks (DBNs) provide a systematic framework for robust online monitoring of dynamic systems. This paper presents an approach for increasing the efficiency of online estimation by partitioning a system DBN into a set of smaller factors, such that estimation algorithms can be applied to each factor independently. Our factoring scheme is based on the analysis of structural observability of the dynamic system. We establish the theoretical background for structural observability and derive an algorithm for generating the factors using structural observability analysis. We present experimental results to demonstrate the effectiveness of our factoring approach for accurate estimation of system behavior. C1 [Roychoudhury, Indranil] NASA, Ames Res Ctr, SGT Inc, Moffett Field, CA 94035 USA. [Biswas, Gautam; Koutsoukos, Xenofon] Vanderbilt Univ, Dept Elect Engn & Comp Sci, Inst Software Integrated Syst, Nashville, TN 37235 USA. RP Roychoudhury, I (reprint author), NASA, Ames Res Ctr, SGT Inc, Moffett Field, CA 94035 USA. EM indranil.roychoudhury@nasa.gov; gautam.biswas@vanderbilt.edu; xenofon.koutsoukos@vanderbilt.edu FU National Science Foundation [CNS- 0615214]; NASA NRA [NNX07AD12A] FX This work was supported by the National Science Foundation under Grant CNS- 0615214 and NASA NRA NNX07AD12A. NR 13 TC 1 Z9 1 U1 0 U2 0 PU IEEE PI NEW YORK PA 345 E 47TH ST, NEW YORK, NY 10017 USA SN 0743-1546 BN 978-1-4244-3872-3 J9 IEEE DECIS CONTR P PY 2009 BP 244 EP 250 DI 10.1109/CDC.2009.5400689 PG 7 WC Automation & Control Systems; Engineering, Electrical & Electronic SC Automation & Control Systems; Engineering GA BA5OA UT WOS:000336893600042 ER PT B AU Tinto, M AF Tinto, M. BE Maleki, L TI SPACE SCIENCE APPLICATIONS OF FREQUENCY STANDARDS AND METROLOGY SO PROCEEDINGS OF THE 7TH SYMPOSIUM FREQUENCY STANDARDS AND METROLOGY LA English DT Proceedings Paper CT 7th Symposium on Frequency Standards and Metrology CY OCT 05-11, 2008 CL Pacific Grove, CA SP Jet Propuls Lab, Aerospace Corporat, Natl Inst Stand & Technol DE Doppler tracking; Space-qualified atomic clocks; Radio science experiments ID GRAVITATIONAL-RADIATION; DOPPLER TRACKING AB We are witnessing the beginning of a new era for space-qualified atomic clocks. These new instruments, characterized by low-mass, low-power consumption, and frequency stabilities comparable to those of ground-based clocks, will allow interplanetary spacecraft radio science experiments at unprecedented Doppler sensitivities. By adding a digital receiver to the onboard instrumentation, it is possible to take advantage of the frequency stability of a space-qualified atomic clock by linearly combining digitally the multi-link Doppler measurements performed on the ground and onboard. This allows one to optimally suppress the frequency fluctuations of the Earth atmosphere, ionosphere and mechanical vibrations of the ground antenna (the dominant Doppler tracking noises) in the resulting Doppler data set. After providing the general expression of the optimal combination of the ground and onboard Doppler data, we apply it, as an example, to interplanetary Doppler tracking searches for gravitational radiation. The resulting estimated sensitivity to milliHertz gravitational waves is about one order of magnitude better than that achievable by traditional two-way coherent Doppler experiments. The Doppler tracking technique discussed in this article can be performed (at minimal additional cost) with future planned interplanetary missions, and extended to other experiments such as spacecraft Doppler tests of relativistic gravity, gravity field measurements, and radio occultations of planetary atmospheres and rings. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Tinto, M (reprint author), CALTECH, Jet Prop Lab, MS 238-737, Pasadena, CA 91109 USA. EM Massimo.Tinto@jpl.nasa.gov NR 20 TC 0 Z9 0 U1 0 U2 0 PU WORLD SCIENTIFIC PUBL CO PTE LTD PI SINGAPORE PA PO BOX 128 FARRER RD, SINGAPORE 9128, SINGAPORE BN 978-981-283-821-6 PY 2009 BP 62 EP 70 PG 9 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA BLM52 UT WOS:000270540200006 ER PT B AU Prestage, JD Chung, S Thompson, R MacNeal, P Le, T AF Prestage, John D. Chung, Sang Thompson, Robert MacNeal, Paul Le, Thanh BE Maleki, L TI SMALL MERCURY MICROWAVE ION CLOCK FOR NAVIGATION AND RADIO-SCIENCE SO PROCEEDINGS OF THE 7TH SYMPOSIUM FREQUENCY STANDARDS AND METROLOGY LA English DT Proceedings Paper CT 7th Symposium on Frequency Standards and Metrology CY OCT 05-11, 2008 CL Pacific Grove, CA SP Jet Propuls Lab, Aerospace Corporat, Natl Inst Stand & Technol AB We have recently completed a breadboard ion-clock physics package based on Hg ions shuttled between a quadrupole and a 16-pole rf trap. With this architecture we have demonstrated short-term stability similar to 1 -2x 10(-13) at 1 second, averaging to 10(-15) at 1 day. This development shows that H-maser quality stabilities can be produced in a small clock package, comparable in size to an ultra-stable quartz oscillator required for holding 1- 10(-13) at 1 second. This performance was obtained in a sealed vacuum configuration where only a getter pump was used to maintain vacuum. Because the tube is scaled, the Hg source and Neon buffer gas are held indefinitely, for the life of the tube. There is no consumption of Hg in this system unlike in a Cs beam tube where lifetime is often limited by Cs depletion. The vacuum tube containing the traps has now been under scaled vacuum conditions for over three years with no measurable degradation of ion trapping lifetimes or clock short-term performance. A 3-liter prototype physics package now in development will be described. C1 [Prestage, John D.; Chung, Sang; Thompson, Robert; MacNeal, Paul; Le, Thanh] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Prestage, JD (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. NR 4 TC 0 Z9 0 U1 0 U2 2 PU WORLD SCIENTIFIC PUBL CO PTE LTD PI SINGAPORE PA PO BOX 128 FARRER RD, SINGAPORE 9128, SINGAPORE BN 978-981-283-821-6 PY 2009 BP 156 EP 165 PG 10 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA BLM52 UT WOS:000270540200016 ER PT B AU Burt, EA Taghavi-Larigani, S Prestage, JD Tjoelker, RL AF Burt, E. A. Taghavi-Larigani, S. Prestage, J. D. Tjoelker, R. L. BE Maleki, L TI COMPENSATED MULTI-POLE MERCURY TRAPPED ION FREQUENCY STANDARD AND STABILITY EVALUATION OF SYSTEMATIC EFFECTS SO PROCEEDINGS OF THE 7TH SYMPOSIUM FREQUENCY STANDARDS AND METROLOGY LA English DT Proceedings Paper CT 7th Symposium on Frequency Standards and Metrology CY OCT 05-11, 2008 CL Pacific Grove, CA SP Jet Propuls Lab, Aerospace Corporat, Natl Inst Stand & Technol AB We have developed a compensated multi-pole Linear Ion Trap Standard (LITS) that eliminates nearly all frequency sensitivity to residual ion number variations. When operated with Hg-199(+), this trapped ion clock has recently demonstrated extremely good stability over a 9-month period. The short-term stability has been measured at 5x10(-14)/tau(1/2) and an upper limit on long-term fractional frequency deviations of <2.7x10(-17)/day was measured in comparison to the laser-cooled primary standards and to the post-processed ultra-stable version of TAI known as TTBIPM using GPS carrier phase time transfer. We have also made a first measurement of the Hg+/Hg collision shift and place a limit of +3.8(7.2)x10(-8)/Pa on the shift constant. C1 [Burt, E. A.; Taghavi-Larigani, S.; Prestage, J. D.; Tjoelker, R. L.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Burt, EA (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. NR 16 TC 0 Z9 0 U1 0 U2 3 PU WORLD SCIENTIFIC PUBL CO PTE LTD PI SINGAPORE PA PO BOX 128 FARRER RD, SINGAPORE 9128, SINGAPORE BN 978-981-283-821-6 PY 2009 BP 321 EP 328 PG 8 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA BLM52 UT WOS:000270540200037 ER PT B AU Burt, EA Taghavi-Larigani, S Lea, SN Prestage, JD Tjoelker, RL AF Burt, E. A. Taghavi-Larigani, S. Lea, S. N. Prestage, J. D. Tjoelker, R. L. BE Maleki, L TI EXPERIMENTS WITH A NEW (201)Hg(+) ION CLOCK SO PROCEEDINGS OF THE 7TH SYMPOSIUM FREQUENCY STANDARDS AND METROLOGY LA English DT Proceedings Paper CT 7th Symposium on Frequency Standards and Metrology CY OCT 05-11, 2008 CL Pacific Grove, CA SP Jet Propuls Lab, Aerospace Corporat, Natl Inst Stand & Technol ID ATOMIC FREQUENCY STANDARDS; FUNDAMENTAL CONSTANTS; TIME-VARIATION; LIMITS AB in this paper we describe a new clock based on (201)Hg(+). All previous mercury ion clocks have been based on (199)Hg(+). We have recently completed construction of the (201)Hg(+) clock and will describe modifications to the design of our existing (199)Hg(+) clocks to accommodate the new isotope. We will also describe initial spectroscopic measurements of the hyperfine manifold, and possible future experiments. One experiment could place a limit on variations in the strong interaction fundamental constant ratio m(q)/Lambda(QCD). C1 [Burt, E. A.; Taghavi-Larigani, S.; Prestage, J. D.; Tjoelker, R. L.] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. RP Burt, EA (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91125 USA. NR 15 TC 1 Z9 1 U1 0 U2 1 PU WORLD SCIENTIFIC PUBL CO PTE LTD PI SINGAPORE PA PO BOX 128 FARRER RD, SINGAPORE 9128, SINGAPORE BN 978-981-283-821-6 PY 2009 BP 358 EP 362 PG 5 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA BLM52 UT WOS:000270540200043 ER PT B AU Dick, J Tu, M Birnbaum, K Strekalov, D Yu, N AF Dick, John Tu, Meirong Birnbaum, Kevin Strekalov, Dmitry Yu, Nan BE Maleki, L TI FUNDAMENTAL NOISE-LIMITED OPTICAL PHASE LOCKING AT FEMTOWATT LIGHT LEVELS SO PROCEEDINGS OF THE 7TH SYMPOSIUM FREQUENCY STANDARDS AND METROLOGY LA English DT Proceedings Paper CT 7th Symposium on Frequency Standards and Metrology CY OCT 05-11, 2008 CL Pacific Grove, CA SP Jet Propuls Lab, Aerospace Corporat, Natl Inst Stand & Technol AB We describe an optical phase lock loop (PLL) designed to recover an optical carrier at powers below one picowatt in a Deep Space optical transponder. Previous low power optical phase lock has been reported with powers down to about 1 pW. We report the demonstration and characterization of the optical phase locking at femtowatt levels. We achieved a phase slip rate below one cycle-slip/second at powers down to 60 femtowatts. This phase slip rate corresponds to a frequency stability Of 1x10(-14) at 1 s, a value better than any frequency standard available today for measuring times equal to a typical two-way delay between Earth and Mars. The PLL shows very robust stability at these power levels. We developed simulation software to optimize parameters of the second order PLL loop in the presence of laser flicker frequency noise and white phase (photon) noise, and verified the software with a white phase noise model by Viterbi. We also demonstrated precise Doppler tracking at femtowatt levels. C1 [Dick, John; Tu, Meirong; Birnbaum, Kevin; Strekalov, Dmitry; Yu, Nan] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Dick, J (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. NR 5 TC 0 Z9 0 U1 1 U2 1 PU WORLD SCIENTIFIC PUBL CO PTE LTD PI SINGAPORE PA PO BOX 128 FARRER RD, SINGAPORE 9128, SINGAPORE BN 978-981-283-821-6 PY 2009 BP 405 EP 416 PG 12 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA BLM52 UT WOS:000270540200050 ER PT B AU Tong, MT Jones, SM Haller, WJ Handschuh, RF AF Tong, Michael T. Jones, Scott M. Haller, William J. Handschuh, Robert F. GP ASME TI ENGINE CONCEPTUAL DESIGN STUDIES FOR A HYBRID WING BODY AIRCRAFT SO PROCEEDINGS OF THE ASME TURBO EXPO 2009, VOL 1 LA English DT Proceedings Paper CT 54th ASME Turbo Expo 2009 CY JUN 08-12, 2009 CL Orlando, FL SP ASME, Int Gas Turbine Inst DE hybrid wing body; fuel burn; noise; emissions AB Worldwide concerns of air quality and climate change have made environmental protection one of the most critical issues in aviation today. NASA's current Fundamental Aeronautics research program is directed at three generations of aircraft in the near, mid and far term, with initial operating capability around 2015, 2020, and 2030, respectively. Each generation has associated goals for fuel burn, NO(x), noise, and field-length reductions relative to today's aircrafts. The research for the 2020 generation is directed at enabling a hybrid wing body (HWB) aircraft to meet NASA's aggressive technology goals. This paper presents the conceptual cycle and mechanical designs of the two engine concepts, podded and embedded systems, which were proposed for a HWB cargo freighter. They are expected to offer significant benefits in noise reductions without compromising the fuel burn. C1 [Tong, Michael T.; Jones, Scott M.; Haller, William J.] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. RP Tong, MT (reprint author), NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. NR 16 TC 0 Z9 0 U1 0 U2 0 PU AMER SOC MECHANICAL ENGINEERS PI NEW YORK PA THREE PARK AVENUE, NEW YORK, NY 10016-5990 USA BN 978-0-7918-4882-1 PY 2009 BP 109 EP 117 PG 9 WC Energy & Fuels; Engineering, Mechanical SC Energy & Fuels; Engineering GA BON15 UT WOS:000277052900011 ER PT B AU Simon, DL Garg, S AF Simon, Donald L. Garg, Sanjay GP ASME TI OPTIMAL TUNER SELECTION FOR KALMAN FILTER-BASED AIRCRAFT ENGINE PERFORMANCE ESTIMATION SO PROCEEDINGS OF THE ASME TURBO EXPO 2009, VOL 1 LA English DT Proceedings Paper CT 54th ASME Turbo Expo 2009 CY JUN 08-12, 2009 CL Orlando, FL SP ASME, Int Gas Turbine Inst AB A linear point design methodology for minimizing the error in on-line Kalman filter-based aircraft engine performance estimation applications is presented. This technique specifically addresses the underdetermined estimation problem, where there are more unknown parameters than available sensor measurements. A systematic approach is applied to produce a model tuning parameter vector of appropriate dimension to enable estimation by a Kalman filter, while minimizing the estimation error in the parameters of interest. Tuning parameter selection is performed using a multi-variable iterative search routine which seeks to minimize the theoretical mean-squared estimation error. This paper derives theoretical Kalman filter estimation error bias and variance values at steady-state operating conditions, and presents the tuner selection routine applied to minimize these values. Results from the application of the technique to an aircraft engine simulation are presented and compared to the conventional approach of tuner selection Experimental simulation results are found to be in agreement with theoretical predictions. The new methodology is shown to yield a significant improvement in on-line engine performance estimation accuracy. C1 [Simon, Donald L.; Garg, Sanjay] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. RP Simon, DL (reprint author), NASA, Glenn Res Ctr, 21000 Brookpk Rd,MS 77-1, Cleveland, OH 44135 USA. NR 9 TC 0 Z9 0 U1 0 U2 0 PU AMER SOC MECHANICAL ENGINEERS PI NEW YORK PA THREE PARK AVENUE, NEW YORK, NY 10016-5990 USA BN 978-0-7918-4882-1 PY 2009 BP 659 EP 671 PG 13 WC Energy & Fuels; Engineering, Mechanical SC Energy & Fuels; Engineering GA BON15 UT WOS:000277052900065 ER PT B AU Shyam, V Ameri, A Luk, DF Chen, JP AF Shyam, Vikram Ameri, Ali Luk, Daniel F. Chen, Jen-Ping GP ASME TI 3-D UNSTEADY SIMULATION OF A MODERN HIGH PRESSURE TURBINE STAGE USING PHASE LAG PERIODICITY: ANALYSIS OF FLOW AND HEAT TRANSFER SO PROCEEDINGS OF THE ASME TURBO EXPO 2009, VOL 3, PTS A AND B LA English DT Proceedings Paper CT 54th ASME Turbo Expo 2009 CY JUN 08-12, 2009 CL Orlando, FL SP ASME, Int Gas Turbine Inst AB Unsteady 3-D RANS simulations have been performed on a highly loaded transonic turbine stage and results are compared to steady calculations as well as experiment. A low Reynolds number k-epsilon turbulence model is employed to provide closure for the RANS system. A phase-lag boundary condition is used in the periodic direction. This allows the unsteady simulation to be performed by using only one blade from each of the two rows. The objective of this paper is to study the effect of unsteadiness on rotor heat transfer and to glean any insight into unsteady flow physics. The role of the stator wake passing on the pressure distribution at the leading edge is also studied. The simulated heat transfer and pressure results agreed favorably with experiment. The time-averaged heat transfer predicted by the unsteady simulation is higher than the heat transfer predicted by the steady simulation everywhere except at the leading edge. The shock structure formed due to stator-rotor interaction was analyzed. Heat transfer and pressure at the hub and casing were also studied. Thermal segregation was observed that leads to the heat transfer patterns predicted by steady and unsteady simulations to be different. C1 [Shyam, Vikram; Ameri, Ali] Ohio State Univ, NASA Glenn Res Ctr, Cleveland, OH USA. RP Shyam, V (reprint author), Ohio State Univ, NASA Glenn Res Ctr, Cleveland, OH USA. NR 20 TC 0 Z9 0 U1 0 U2 0 PU AMER SOC MECHANICAL ENGINEERS PI NEW YORK PA THREE PARK AVENUE, NEW YORK, NY 10016-5990 USA BN 978-0-7918-4884-5 PY 2009 BP 1039 EP 1049 PG 11 WC Energy & Fuels; Engineering, Mechanical SC Energy & Fuels; Engineering GA BON21 UT WOS:000277056900091 ER PT J AU Urzay, J Nayagam, V Williams, FA AF Urzay, Javier Nayagam, Vedha Williams, Forman A. TI Diffusion-flame extinction on a rotating porous-disk burner SO PROCEEDINGS OF THE COMBUSTION INSTITUTE LA English DT Article DE Laminar flames; Nonpremixed combustion; Asymptotic analysis; Extinction ID ASYMPTOTIC STRUCTURE; EDGE-FLAMES; COUNTERFLOW; DYNAMICS AB Flames advected by swirling flows are subject to large strain rates that may cause local extinction. In this investigation, a porous-disk burner is spun at a constant angular velocity in an otherwise quiescent oxidizing atmosphere. Gaseous methane is injected through the disk pores and burns in a flat diffusion flame adjacent to the disk, resulting in a variety of nonpremixed flame patterns for different combinations of the angular velocity and fuel flow rate. The method of activation-energy asymptotics is employed to address the transition from conditions under which a diffusion flame envelops the entire disk to conditions under which diffusion flames are present over only part of the disk, leading to the presence of edge flames. An expression for the extinction Damkohler number as a function of the fuel flow rate and angular velocity is derived and compared with experiments. Agreement is favorable when parameters for a one-step model of methane combustion are employed. (C) 2009 The Combustion Institute. Published by Elsevier Inc. All rights reserved. C1 [Urzay, Javier; Williams, Forman A.] Univ Calif San Diego, Dept Mech & Aerosp Engn, La Jolla, CA 92093 USA. [Urzay, Javier; Williams, Forman A.] Univ Calif San Diego, Energy Res Ctr, La Jolla, CA 92093 USA. [Nayagam, Vedha] NASA, Glenn Res Ctr, Natl Ctr Space Explorat Res, Cleveland, OH 44135 USA. RP Urzay, J (reprint author), Univ Calif San Diego, Dept Mech & Aerosp Engn, 9500 Gilman Dr, La Jolla, CA 92093 USA. EM jurzay@ucsd.edu RI Urzay, Javier /H-6029-2013 NR 13 TC 2 Z9 2 U1 0 U2 2 PU ELSEVIER SCIENCE INC PI NEW YORK PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA SN 1540-7489 J9 P COMBUST INST JI Proc. Combust. Inst. PY 2009 VL 32 BP 1219 EP 1226 DI 10.1016/j.proci.2008.06.016 PG 8 WC Thermodynamics; Energy & Fuels; Engineering, Chemical; Engineering, Mechanical SC Thermodynamics; Energy & Fuels; Engineering GA 427CG UT WOS:000264756800140 ER PT J AU Bellan, J Selle, LC AF Bellan, J. Selle, L. C. TI Large Eddy Simulation composition equations for single-phase and two-phase fully multicomponent flows SO PROCEEDINGS OF THE COMBUSTION INSTITUTE LA English DT Article DE Multicomponent LES equations ID DIRECT NUMERICAL-SIMULATION; PLANE MIXING LAYER; EVAPORATING DROPS; MIXTURES; TURBULENCE; LADEN; COMPONENTS; PARTICLES; NUMBER; MODEL AB The Large Eddy Simulation (LES) equations for multicomponent (MC) fuel single-phase (SP) flow and two-phase (TP) flow with phase change are derived from the Direct Numerical Simulation (DNS) equations by filtering the DNS equations using a top-hat filter. Additional to the equations solved for single-component (SC) fuels, composition equations enter the formulation. The species composition is represented through a Probability Distribution Function (PDF), and DNS equations for the PDF moments are solved to find the composition. The TP filtered equations contain three categories of subgrid-scale (SGS) terms: ( 1) SGS-flux terms, (2) filtered Source terms (FSTs) and (3) terms representing the 'LES assumptions'. For SP flows no FSTs exist. The SGS terms in the LES equations must be either shown negligible or modeled. It is shown that for the composition equations, two equivalent forms of the DNS equations lead to two non-equivalent forms of the LES equations. Criteria are proposed to select the form best suited for LES. These criteria are used in conjunction with evaluations based oil a DNS database portraying mixing and phase change, and lead to choosing one of the LES forms which satisfies all criteria. It is shown that the LES assumptions lead to additional SGS terms which require modeling. Further considerations are made for reactive flows. (C) 2009 Published by Elsevier Inc. on behalf of The Combustion Institute. C1 [Bellan, J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Bellan, J.; Selle, L. C.] CALTECH, Dept Mech Engn, Pasadena, CA 91125 USA. RP Bellan, J (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr,M-S 125-109, Pasadena, CA 91109 USA. EM Josette.Bellan@jpl.nasa.gov RI Selle, Laurent/I-6369-2013 OI Selle, Laurent/0000-0002-5997-3646 FU Jet Propulsion Laboratory (JPL); California Institute of Technology (Caltech); American Chemical Society FX This study was conducted at the Jet Propulsion Laboratory (JPL), California Institute of Technology (Caltech), under the partial sponsorship of the Donors of The Petroleum Research Fund administered by the American Chemical Society through a grant (to J.B.) for Caltech Post Doctoral Fellow (L.S.) Support, and of the Air Force Research Laboratory. Wright Patterson Air Force Base with Dr. Tim Edwards as technical monitor. Computational resources were provided by the supercomputing facility at JPL. NR 22 TC 4 Z9 4 U1 0 U2 9 PU ELSEVIER SCIENCE INC PI NEW YORK PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA SN 1540-7489 J9 P COMBUST INST JI Proc. Combust. Inst. PY 2009 VL 32 BP 2239 EP 2246 DI 10.1016/j.proci.2008.06.005 PG 8 WC Thermodynamics; Energy & Fuels; Engineering, Chemical; Engineering, Mechanical SC Thermodynamics; Energy & Fuels; Engineering GA 427CH UT WOS:000264756900072 ER PT J AU Olson, SL Miller, FJ AF Olson, S. L. Miller, F. J. TI Experimental comparison of opposed and concurrent flame spread in a forced convective microgravity environment SO PROCEEDINGS OF THE COMBUSTION INSTITUTE LA English DT Article DE Opposed flame spread; Concurrent flame spread; Microgravity; Normoxic conditions; Recirculation cell ID THIN; FLOW; FUEL AB Flame spread experiments in both concurrent and opposed flow have been carried out in a 5.18-s drop tower with a thin cellulose fuel. Flame spread rate and flame length have been measured over a range 0-30 cm/s forced flow (in both directions), 3.6-14.7 psia, and oxygen mole fractions 0.24-0.85 in nitrogen. Results are presented for each of the three variables independently to elucidate their individual effects, with special emphasis on pressure/oxygen combinations that result in earth-equivalent oxygen partial pressures (normoxic conditions). Correlations using all three variables combined into a single parameter to predict flame spread rate are presented. The correlations are used to demonstrate that opposed flow flames in typical spacecraft ventilation flows (5-20 cm/s) spread faster than concurrent flow flames under otherwise similar conditions (pressure, oxygen concentration) in nearly all spacecraft atmospheres. This indicates that in the event of an actual fire aboard a spacecraft, the fire is likely to grow most quickly in the opposed mode as the upstream flame spreads faster and the downstream flame is inhibited by the vitiated atmosphere produced by the upstream flame. Additionally, an interesting phenomenon was observed at intermediate values of concurrent forced flow velocity where flow/flame interactions produced a recirculation downstream of the flame, which allowed an opposed flow leading edge to form there. Published by Elsevier Inc. on behalf of The Combustion Institute. C1 [Olson, S. L.] NASA, Glenn Res Ctr Lewis Field, Cleveland, OH 44135 USA. [Miller, F. J.] San Diego State Univ, Dept Mech Engn, San Diego, CA 92182 USA. RP Olson, SL (reprint author), NASA, Glenn Res Ctr Lewis Field, MS 77-5, Cleveland, OH 44135 USA. EM sandra.l.olson@nasa.gov FU NASA's Fire Prevention, Detection, and Suppression Program FX The research at NASA Glenn's Zero Gravity Research Facility was supported by NASA's Fire Prevention, Detection, and Suppression Program. We thank the personnel of the NASA Glenn Zero Gravity Research Facility for upgrading the experiment apparatus and conducting the drop testing. We thank Glenn's Spacecraft Fire Prevention team for reviewing this work. NR 21 TC 10 Z9 12 U1 2 U2 12 PU ELSEVIER SCIENCE INC PI NEW YORK PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA SN 1540-7489 J9 P COMBUST INST JI Proc. Combust. Inst. PY 2009 VL 32 BP 2445 EP 2452 DI 10.1016/j.proci.2008.05.081 PG 8 WC Thermodynamics; Energy & Fuels; Engineering, Chemical; Engineering, Mechanical SC Thermodynamics; Energy & Fuels; Engineering GA 427CH UT WOS:000264756900097 ER PT J AU McAllister, S Fernandez-Pello, C Urban, D Ruff, G AF McAllister, Sara Fernandez-Pello, Carlos Urban, David Ruff, Gary TI Piloted ignition delay of PMMA in space exploration atmospheres SO PROCEEDINGS OF THE COMBUSTION INSTITUTE LA English DT Article DE Piloted ignition; Pressure; Oxygen; Exploration atmosphere ID EXTINCTION; OXYGEN; FUELS AB In order to reduce the risk of decompression sickness associated with extra-vehicular activity (EVA), NASA is designing the next generation of exploration vehicles and habitats with a different, cabin environment than used previously. The proposed environment uses a total cabin pressure of 52.7-58.6 kPa with all oxygen concentration of 30-34% by volume and was chosen with material flammability in mind. Because materials may burn differently under these conditions and there is little information oil how this new environment affects the flammability of the materials onboard, it is important to conduct material flammability experiments at the intended exploration atmosphere. One method to evaluate material flammability is by its ease of ignition. To this end, piloted ignition delay tests were conducted in the Forced Ignition and Spread Test (FIST) apparatus Subject to this new environment. In these tests, polymethylmethacylate (PMMA) was exposed to a range of oxidizer flow velocities and externally applied heat fluxes. Tests were conducted for a baseline case of normal pressure and oxygen concentration, low pressure (58.6 kPa) with normal oxygen (21%), and low pressure with 32% oxygen concentration conditions to determine the individual effect of pressure and the combined effect of pressure and oxygen concentration oil the ignition delay. It was found that reducing the pressure while keeping the oxygen concentration at 21%, reduced the ignition time by 17% on average. Increasing the oxygen concentration at low pressures reduced the ignition time by an additional 10%. It was also noted that the critical heat flux for ignition decreases at exploration atmospheres. These results show that tests conducted in standard atmospheric conditions will underpredict the ignition of materials intended for use on spacecraft and that, at these conditions, materials are more susceptible to ignition than at current spacecraft atmospheres. (C) 2009 The Combustion Institute. Published by Elsevier Inc. All rights reserved. C1 [McAllister, Sara; Fernandez-Pello, Carlos] Univ Calif Berkeley, Dept Mech Engn, Berkeley, CA 94720 USA. [Urban, David; Ruff, Gary] NASA, John H Glenn Res Ctr, Cleveland, OH 44256 USA. RP McAllister, S (reprint author), Univ Calif Berkeley, Dept Mech Engn, 60A Hesse Hall,Mailstop 1740, Berkeley, CA 94720 USA. EM smcalliser@berkeley.edu FU NASA [NNC-05GA02G] FX This work was supported by NASA Grant NNC-05GA02G. The authors thank Janice Lai, Sarah Scott, and Amelia Ramirez-Correa for their indispensable assistance running the experiments: Chris Lautenberger for his insightful (discussions and input; and Paul Ferkul for his unbiased review of the manuscript. NR 26 TC 12 Z9 12 U1 0 U2 5 PU ELSEVIER SCIENCE INC PI NEW YORK PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA SN 1540-7489 J9 P COMBUST INST JI Proc. Combust. Inst. PY 2009 VL 32 BP 2453 EP 2459 DI 10.1016/j.proci.2008.05.076 PG 7 WC Thermodynamics; Energy & Fuels; Engineering, Chemical; Engineering, Mechanical SC Thermodynamics; Energy & Fuels; Engineering GA 427CH UT WOS:000264756900098 ER PT J AU Takahashi, F Katta, VR AF Takahashi, Fumiaki Katta, Viswanath R. TI Extinguishment of diffusion flames around a cylinder in a coaxial air stream with dilution or water mist SO PROCEEDINGS OF THE COMBUSTION INSTITUTE LA English DT Article DE Fire suppression; Diffusion flame extinguishment; PMMA; Carbon dioxide; Water mist ID NON-PREMIXED FLAMES; CUP-BURNER FLAMES; SUPPRESSION EFFECTIVENESS; DROPLETS AB Extinguishment of methane and polymethylmethacrylate(PMMA) diffusion flames by gaseous and water mist fire-extinguishing agents has been studied experimentally and computationally using a cylindrical burner inserted downwardly into all upward coaxial air stream. Transient computations were performed for methane flames with full chemistry and a simple water- mist model to reveal the flame Structure and Suppression processes. For methane, as a gaseous agent (CO(2) or N(2)) or water mist (:approximate to 35 mu m number mean diameter) was added incrementally to the air stream: (1) a diffusion flame enveloping a Porous bottom surface or the cylinder extinguished first, resulting in a flame with its base(edge) anchored at the leading edge of the side of the porous cylinder; and (2) the flame base oscillated, detached, drifted downstream, and extinguished eventually. For PMMA. the flame base attached to the fuel Surface more closely than methane flames until detachment led to blowoff. The volume fractions of CO(2) or N(2) in the oxidizer stream at detachment and extinguishment were independent (or mild functions) of the mean oxidizer velocity (U(ox)). In computations, the initial envelope flame extinction led to extinguishment at the limits between the measured detachment and extinguishing conditions. The measured water flow rate at extinguishment was independent or U(ox); thus, the water mass fraction decreased dramatically with increasing U(ox), suggesting that the water mist was transported to the flame zone independently of the air flow. The calculated water mass fraction at extinguishment, by contrast, decreased only mildly with U(ox) because water mist was modeled as a gaseous species. The computation of the near-limit flames revealed that: (1) extinguishment occurred when the peak temperature decreased to approximate to 1600 K: (2) adding CO(2) or H(2)O exhibited chemical effects oil the flame structure; and (3) the stagnation-point-flow structure was nearly identical to that of a near-extinction counterflow diffusion flame. (c) 2009 The Combustion Institute. Published by Elsevier Inc. All rights reserved. C1 [Takahashi, Fumiaki] NASA, Natl Ctr Space Explorat Res Fluids & Combust, Glenn Res Ctr, Cleveland, OH 44135 USA. [Katta, Viswanath R.] Innovat Sci Solut Inc, Dayton, OH 45440 USA. RP Takahashi, F (reprint author), NASA, Natl Ctr Space Explorat Res Fluids & Combust, Glenn Res Ctr, 21000 Brookpk Rd,MS 110-3, Cleveland, OH 44135 USA. EM fxt13@case.edu FU Office of Biological and Physical Research and the Fire Prevention, Detection, and Suppression program; Exploration Technology Development Program Office; National Aeronautics and Space Agency, Washington, DC FX This research was supported by the Office of Biological and Physical Research and the Fire Prevention, Detection, and Suppression program in the Exploration Technology Development Program Office, National Aeronautics and Space Agency, Washington, DC. NR 29 TC 16 Z9 18 U1 2 U2 7 PU ELSEVIER SCIENCE INC PI NEW YORK PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA SN 1540-7489 J9 P COMBUST INST JI Proc. Combust. Inst. PY 2009 VL 32 BP 2615 EP 2623 DI 10.1016/j.proci.2008.05.028 PG 9 WC Thermodynamics; Energy & Fuels; Engineering, Chemical; Engineering, Mechanical SC Thermodynamics; Energy & Fuels; Engineering GA 427CH UT WOS:000264756900118 ER PT B AU DellaCorte, C AF DellaCorte, Christopher GP ASME TI TECHNICAL DEVELOPMENT PATH FOR FOIL GAS BEARINGS SO PROCEEDINGS OF THE STLE/ASME INTERNATIONAL JOINT TRIBOLOGY CONFERENCE 2008 LA English DT Proceedings Paper CT STLE/ASME 2008 International Joint Tribology Conference CY OCT 20-22, 2008 CL Miami, FL SP Soc Tribologists & Lubricat Engineers, Amer Soc Mech Engineers AB Foil gas bearings are in widespread commercial use in air cycle machines, turbocompressors and microturbine generators and are emerging in more challenging applications such as turbochargers, auxiliary power units and propulsion gas turbines. Though not well known, foil bearing technology is well over fifty years old. Recent technological developments indicate that their full potential has yet to be realized. This paper investigates the key technological developments that have characterized foil bearing advances. It is expected that a better understanding of foil gas bearing development path will aid in future development and progress towards more advanced applications. C1 NASA, Glenn Res Ctr, Cleveland, OH USA. RP DellaCorte, C (reprint author), NASA, Glenn Res Ctr, Cleveland, OH USA. NR 20 TC 0 Z9 0 U1 0 U2 0 PU AMER SOC MECHANICAL ENGINEERS PI NEW YORK PA THREE PARK AVENUE, NEW YORK, NY 10016-5990 USA BN 978-0-7918-4336-9 PY 2009 BP 299 EP 302 PG 4 WC Engineering, Mechanical; Nanoscience & Nanotechnology; Materials Science, Multidisciplinary; Physics, Applied SC Engineering; Science & Technology - Other Topics; Materials Science; Physics GA BJJ09 UT WOS:000266325200079 ER PT B AU Bruckner, RJ AF Bruckner, Robert J. GP ASME TI EVALUATION OF SUPERCRITICAL CARBON DIOXIDE FOR USE IN FLUID FILM BEARINGS FOR PROCESS FLUID LUBRICATED MACHINES SO PROCEEDINGS OF THE STLE/ASME INTERNATIONAL JOINT TRIBOLOGY CONFERENCE 2008 LA English DT Proceedings Paper CT STLE/ASME 2008 International Joint Tribology Conference CY OCT 20-22, 2008 CL Miami, FL SP Soc Tribologists & Lubricat Engineers, Amer Soc Mech Engineers C1 NASA, Glenn Res Ctr, Cleveland, OH USA. RP Bruckner, RJ (reprint author), NASA, Glenn Res Ctr, Cleveland, OH USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU AMER SOC MECHANICAL ENGINEERS PI NEW YORK PA THREE PARK AVENUE, NEW YORK, NY 10016-5990 USA BN 978-0-7918-4336-9 PY 2009 BP 407 EP 409 PG 3 WC Engineering, Mechanical; Nanoscience & Nanotechnology; Materials Science, Multidisciplinary; Physics, Applied SC Engineering; Science & Technology - Other Topics; Materials Science; Physics GA BJJ09 UT WOS:000266325200106 ER PT B AU Dimofte, F Ene, NM Oswald, FB AF Dimofte, Florin Ene, Nicoleta M. Oswald, Fred B. GP ASME TI OIL WAVE JOURNAL BEARING STEADY-STATE DATA FROM A NEW TEST RIG SO PROCEEDINGS OF THE STLE/ASME INTERNATIONAL JOINT TRIBOLOGY CONFERENCE 2008 LA English DT Proceedings Paper CT STLE/ASME 2008 International Joint Tribology Conference CY OCT 20-22, 2008 CL Miami, FL SP Soc Tribologists & Lubricat Engineers, Amer Soc Mech Engineers AB An oil lubricated wave bearing has been tested on a new rig for fluid film journal bearings at NASA Glenn Research Center in Cleveland, Ohio, USA. The tests are intended to evaluate the rig possibilities of running without misaligmnent. Data recorded under steady-state conditions included oil flow rate, input, output and oil supply temperatures, and shaft position. Two sets of data were collected: i) by varying the load to 9000 N at a constant shaft rotation speed of 8,000 RPM and ii) by varying the speed from 9,000 to 12,000 RPM at constant load of 6,700 N. The temperatures of the metal sleeves were also recorded. Vibration levels at four locations were displayed and recorded. These measurements indicated that damping from the wave bearings provides significant attenuation of the vibration generated by the air turbine that drives the rig. C1 [Dimofte, Florin] Univ Toledo, NASA, Glenn Res Ctr, Cleveland, OH USA. RP Dimofte, F (reprint author), Univ Toledo, NASA, Glenn Res Ctr, Cleveland, OH USA. NR 3 TC 0 Z9 0 U1 0 U2 0 PU AMER SOC MECHANICAL ENGINEERS PI NEW YORK PA THREE PARK AVENUE, NEW YORK, NY 10016-5990 USA BN 978-0-7918-4336-9 PY 2009 BP 415 EP 417 PG 3 WC Engineering, Mechanical; Nanoscience & Nanotechnology; Materials Science, Multidisciplinary; Physics, Applied SC Engineering; Science & Technology - Other Topics; Materials Science; Physics GA BJJ09 UT WOS:000266325200108 ER PT J AU Meyyappan, M AF Meyyappan, M. TI Catalyzed chemical vapor deposition of one-dimensional nanostructures and their applications SO PROGRESS IN CRYSTAL GROWTH AND CHARACTERIZATION OF MATERIALS LA English DT Review DE Nanostructures; One-dimensional nanomaterials; Low temperature plasma; Catalyzed growth; Vapor-liquid-solid technique; Chemical vapor deposition ID CARBON NANOTUBE GROWTH; MULTILAYERED METAL-CATALYSTS; RANDOM-ACCESS MEMORY; GERMANIUM NANOWIRES; SILICON NANOWIRES; SEMICONDUCTOR NANOWIRES; THERMOELECTRIC FIGURE; SELECTIVE GROWTH; CRYSTAL-GROWTH; GAN NANOWIRES AB This article reviews progress in the growth of one-dimensional nanomaterials such as carbon nanotubes and inorganic nanowires. Catalyzed chemical vapor deposition has been the preferred method to grow these materials for various applications requiring controlled growth on patterned and unpatterned substrates. Both thermal and plasma chemical vapor deposition techniques have been widely used in the case of carbon nanotubes. In addition to the discussion on growth, a review of applications for one-dimensional nanostructures and future directions is provided. Published by Elsevier Ltd. C1 NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Meyyappan, M (reprint author), NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. EM m.meyyappan@nasa.gov NR 94 TC 19 Z9 19 U1 5 U2 29 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0960-8974 J9 PROG CRYST GROWTH CH JI Prog. Cryst. Growth Charact. Mater. PY 2009 VL 55 IS 1-2 BP 1 EP 21 DI 10.1016/j.pcrysgrow.2009.01.001 PG 21 WC Crystallography; Materials Science, Characterization & Testing SC Crystallography; Materials Science GA 440VD UT WOS:000265726900001 ER PT J AU Phillips, AJ Brodeur, RD Suntsov, AV AF Phillips, A. Jason Brodeur, Richard D. Suntsov, Andrey V. TI Micronekton community structure in the epipelagic zone of the northern California Current upwelling system SO PROGRESS IN OCEANOGRAPHY LA English DT Review DE Pacific Ocean; Marine micronekton; Lanternfish; Community composition; Species diversity; California Current ID VERTICAL-DISTRIBUTION; STENOBRACHIUS-LEUCOPSARUS; FISHERIES MANAGEMENT; FEEDING-HABITS; COASTAL OCEAN; OREGON COAST; ECOSYSTEM; PACIFIC; USA; MYCTOPHIDAE AB Spatial and temporal variability in the micronekton community and in oceanographic conditions were evaluated from nighttime midwater trawl samples collected between Heceta Head, Oregon (44.0 degrees N) and Willapa Bay, Washington (46.6 degrees N). Collections from 13 cruises (176 trawls) from 2004 to 2006 yielded over 17,000,000 micronekton individuals (350,000 excluding euphausiids), representing 76 taxa and 43 families. The community was numerically dominated by euphausiids, followed in decreasing order by midwater shrimp (Sergestes similis), lanternfishes (Myctophidae), late larval/juvenile rockfishes (Sebastes spp.), age-0 Pacific hake (Merluccius productus), and pelagic squid (Abraliopsis felis). We used cluster analysis, ordinations, multi-response permutation procedures (MRPP), and indicator species analysis (ISA) to examine community structure of the 28 dominant taxa. Ordination and cluster results indicated that distance from shore and sea-floor depth best characterized habitats used by different assemblages of the micronekton community. Temperature and salinity at various depths influenced community structure to a lesser extent, along with Ekman transport. MRPP and ISA results indicated that nearly all dominant taxa were associated with cross-shelf gradients. Based upon a comparison between historical samples collected in 1976 and 1981 and comparable trawls from this survey, distinct decadal differences among micronektonic fish assemblages were observed, including more juvenile flatfishes and rockfishes but a lower diversity of mesopelagic fishes, which may be related to interdecadal environmental changes between the two time periods. This study represents the first examination of the relationships between both vertebrate and invertebrate members of the epipelagic nekton community. (C) 2008 Elsevier Ltd. All rights reserved. C1 [Phillips, A. Jason] Oregon State Univ, Cooperat Inst Marine Resources Studies, Newport, OR 97365 USA. [Brodeur, Richard D.; Suntsov, Andrey V.] NW Fisheries Sci Ctr, Natl Marine Fisheries Serv, Newport, OR 97365 USA. RP Phillips, AJ (reprint author), 104 COAS Adm Bldg, Corvallis, OR 97331 USA. EM jphillip@coas.oregonstate.edu FU NCAA Northwest Fisheries Science Center FX We wish to thank Toby Auth, Paul Peterson, Jesse Lamb, Paul Bentley, Bob Emmett, and the crew of the research and fishing vessels that participated in the cruises and in processing of samples in the laboratory. We would like to thank Bill Pearcy for providing unpublished data. Also, we would like to thank Bill Pearcy, Toby Auth, Ed Casillas and Doug Reese for comments on earlier versions of this manuscript. Funding for the collection and analysis of the data comes from the NCAA Northwest Fisheries Science Center and NCAA's Stock Assessment Improvement Program. NR 66 TC 12 Z9 12 U1 2 U2 18 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0079-6611 J9 PROG OCEANOGR JI Prog. Oceanogr. PD JAN-FEB PY 2009 VL 80 IS 1-2 BP 74 EP 92 DI 10.1016/j.pocean.2008.12.001 PG 19 WC Oceanography SC Oceanography GA 425SO UT WOS:000264657600004 ER PT S AU Golden, JL Koontz, SL Christiansen, EL Graves, RF Lorenz, MJ Alred, JW O'Rourke, MJE AF Golden, Johnny L. Koontz, Steven L. Christiansen, Eric L. Graves, Russell F. Lorenz, Mary J. Alred, John W. O'Rourke, Mary Jane E. BE Kleiman, JI TI Spacecraft Materials in the Space Flight Environment: International Space Station - May 2002 to May 2008 SO PROTECTION OF MATERIALS AND STRUCTURES FROM SPACE ENVIRONMENT SE AIP Conference Proceedings LA English DT Proceedings Paper CT 9th International Conference on Protection of Materials and Structures from Space Environment CY MAY 20-23, 2008 CL Toronto, CANADA SP Canadian Space Agcy, Montana State Univ, Univ Toronto Inst Aerospac Studies, Integr Testing Lab ID LOW-EARTH-ORBIT; FIGURE; MERIT AB The performance of ISS spacecraft materials and systems on prolonged exposure to the low-Earth orbit (LEO) space flight are reported in this paper. In-flight data, flight crew observations, and the results of ground-based test and analysis directly supporting programmatic and operational decision-making are described. The space flight environments definitions (both natural and induced) used for ISS design, material selection, and verification testing are shown, in most cases, to be more severe than the actual flight environment accounting, in parts for the outstandmig performance of ISS as a long mission duration spacecraft. No significant ISS material or system failures have been attributed to spacecraft-environments interactions. Nonetheless, ISS materials and systems performance data is contributing to our understanding of spacecraft material interactions with the spaceflight environment so as to reduce cost and risk for future spaceflight projects and programs. C1 [Golden, Johnny L.; Lorenz, Mary J.] Boeing ISS Mat & Proc, Mail Code HB3-20,13100 Space Ctr Blvd, Houston, TX 77059 USA. [Koontz, Steven L.; Alred, John W.; O'Rourke, Mary Jane E.] NASA, Johnson Space Ctr, Struct Engn Div, Houston, TX 77058 USA. [Christiansen, Eric L.] NASA, Johnson Space Ctr, Solar Syst Explorat Div, Houston, TX 77058 USA. [Graves, Russell F.] Boeing ISS Struct Mechanisms, Houston, TX 77059 USA. RP Golden, JL (reprint author), Boeing ISS Mat & Proc, Mail Code HB3-20,13100 Space Ctr Blvd, Houston, TX 77059 USA. EM johny.l.golden@boeing.com NR 81 TC 2 Z9 2 U1 0 U2 0 PU AMER INST PHYSICS PI MELVILLE PA 2 HUNTINGTON QUADRANGLE, STE 1NO1, MELVILLE, NY 11747-4501 USA SN 0094-243X BN 978-0-7354-0619-3 J9 AIP CONF PROC PY 2009 VL 1087 BP 3 EP + PG 5 WC Engineering, Aerospace SC Engineering GA BIX44 UT WOS:000263582700001 ER PT S AU Stambler, AH Inoshita, KE Roberts, LM Barbagallo, CE de Groh, KK Banks, BA AF Stambler, Arielle H. Inoshita, Karen E. Roberts, Lily M. Barbagallo, Claire E. de Groh, Kim K. Banks, Bruce A. BE Kleiman, JI TI Ground-Laboratory to In-Space Atomic Oxygen Correlation for the PEACE Polymers SO PROTECTION OF MATERIALS AND STRUCTURES FROM SPACE ENVIRONMENT SE AIP Conference Proceedings LA English DT Proceedings Paper CT 9th International Conference on Protection of Materials and Structures from Space Environment CY MAY 20-23, 2008 CL Toronto, CANADA SP Canadian Space Agcy, Montana State Univ, Univ Toronto Inst Aerospac Studies, Integr Testing Lab AB The Materials International Space Station Experiment 2 (MISSE 2) Polymer Erosion and Contamination Experiment (PEACE) polymers were exposed to the environment of low Earth orbit (LEO) for 3.95 years from 2001 to 2005. There were forty-one different PEACE polymers, which were flown on the exterior of the International Space Station (ISS) in order to determine their atomic oxygen erosion yields. In LEO, atomic oxygen is an environmental durability threat, particularly for long duration mission exposures. Although space flight experiments, such as the MISSE 2 PEACE experiment, are ideal for determining LEO environmental durability of spacecraft materials, ground-laboratory testing is often relied upon for durability evaluation and prediction. Unfortunately, significant differences exist between LEO atomic oxygen exposure and atomic oxygen exposure in ground-laboratory facilities. These differences include variations in species, energies, thermal exposures and radiation exposures, all of which may result in different reactions and erosion rates. In an effort to improve the accuracy of ground-based durability testing, ground-l ab oratory to in-space atomic oxygen correlation experiments have been conducted. In these tests, the atomic oxygen erosion yields of the PEACE polymers were determined relative to Kapton H using a radio-frequency (RF) plasma asher (operated on air). The asher erosion yields were compared to the MISSE 2 PEACE erosion yields to determine the correlation between erosion rates in the two environments. This paper provides a summary of the MISSE 2 PEACE experiment; it reviews the specific polymers tested as well as the techniques used to determine erosion yield in the asher, and it provides a correlation between the space and ground-laboratory erosion yield values. Using the PEACE polymers' asher to in-space erosion yield ratios will allow more accurate in-space materials performance predictions to be made based on plasma asher durability evaluation. C1 [Stambler, Arielle H.; Inoshita, Karen E.; Roberts, Lily M.; Barbagallo, Claire E.] Hathaway Brown Sch, 19600 N Pk Blvd, Shaker Hts, OH 44122 USA. [de Groh, Kim K.] NASA, Lewis Res Ctr, Cleveland, OH 44135 USA. [Banks, Bruce A.] NASA, Lewis Res Ctr, Consultant Alphaport InC, Cleveland, OH 44135 USA. RP Stambler, AH (reprint author), Hathaway Brown Sch, 19600 N Pk Blvd, Shaker Hts, OH 44122 USA. EM kim.k.degroh@nasa.gov; bruce.a.banks@nasa.gov NR 13 TC 3 Z9 3 U1 0 U2 1 PU AMER INST PHYSICS PI MELVILLE PA 2 HUNTINGTON QUADRANGLE, STE 1NO1, MELVILLE, NY 11747-4501 USA SN 0094-243X BN 978-0-7354-0619-3 J9 AIP CONF PROC PY 2009 VL 1087 BP 51 EP + PG 3 WC Engineering, Aerospace SC Engineering GA BIX44 UT WOS:000263582700003 ER PT S AU Kauder, LR AF Kauder, Lonny R. BE Kleiman, JI TI An Improved Formulation for Calorimetric Emittance Testing of Spacecraft Thermal Control Coatings SO PROTECTION OF MATERIALS AND STRUCTURES FROM SPACE ENVIRONMENT SE AIP Conference Proceedings LA English DT Proceedings Paper CT 9th International Conference on Protection of Materials and Structures from Space Environment CY MAY 20-23, 2008 CL Toronto, CANADA SP Canadian Space Agcy, Montana State Univ, Univ Toronto Inst Aerospac Studies, Integr Testing Lab AB Spacecraft often rely heavily on passive thermal control to maintain operating temperature. An important parameter in the spacecraft heat balance equation is the emittance of thermal control coatings as a function of coating temperature. One method for determining the emittance of spacecraft thermal control from elevated temperature to cryogenic temperatures relies on a calorimetric technique. The fundamental equation governing this test method can be found in numerous places in the literature and although it generally provides reasonable results, its formulation is based on a conceptual flaw that only becomes apparent when the sample temperature approaches the wall temperature during testing. This paper investigates the cause for this error and develops the correct formulation for calorimetric emittance testing. Experimental data will also be presented that illustrates the difference between the two formulations and the resulting difference in the calculated emittance. C1 NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Kauder, LR (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. NR 6 TC 1 Z9 1 U1 0 U2 0 PU AMER INST PHYSICS PI MELVILLE PA 2 HUNTINGTON QUADRANGLE, STE 1NO1, MELVILLE, NY 11747-4501 USA SN 0094-243X BN 978-0-7354-0619-3 J9 AIP CONF PROC PY 2009 VL 1087 BP 117 EP 123 PG 7 WC Engineering, Aerospace SC Engineering GA BIX44 UT WOS:000263582700010 ER PT S AU Finckenor, M AF Finckenor, Miria BE Kleiman, JI TI MISSE Thermal Control Materials with Comparison to Previous Flight SO PROTECTION OF MATERIALS AND STRUCTURES FROM SPACE ENVIRONMENT SE AIP Conference Proceedings LA English DT Proceedings Paper CT 9th International Conference on Protection of Materials and Structures from Space Environment CY MAY 20-23, 2008 CL Toronto, CANADA SP Canadian Space Agcy, Montana State Univ, Univ Toronto Inst Aerospac Studies, Integr Testing Lab AB Many different passive thermal control materials were flown as part of the Materials on International Space Station Experiment, including inorganic coatings, anodized aluminum, and multi-layer insulation materials. These and other material samples were exposed to the low Earth orbital environment of atomic oxygen, ultraviolet radiation, thermal cycling, and hard vacuum, though atomic oxygen exposure was limited for some samples. Materials flown on MISSE-1 and MISSE-2 were exposed to the space environment for nearly four years. Materials flown on MISSE-3, MISSE-4, and MISSE-5 were exposed to the space environment for one year. Solar absorptance, infrared emittance, and mass measurements indicate the durability of these materials to withstand the space environment. Effects of short duration versus long duration exposure on ISS are explored, as well as comparable data from previous flight experiments, such as the Passive Optical Sample Assembly (POSA), Optical Properties Monitor (OPM), and Long Duration Exposure Facility (LDEF). C1 NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA. RP Finckenor, M (reprint author), NASA, George C Marshall Space Flight Ctr, Mail Code EM50, Huntsville, AL 35812 USA. EM miria.finckenor@nasa.gov NR 10 TC 1 Z9 1 U1 0 U2 2 PU AMER INST PHYSICS PI MELVILLE PA 2 HUNTINGTON QUADRANGLE, STE 1NO1, MELVILLE, NY 11747-4501 USA SN 0094-243X BN 978-0-7354-0619-3 J9 AIP CONF PROC PY 2009 VL 1087 BP 241 EP 248 PG 8 WC Engineering, Aerospace SC Engineering GA BIX44 UT WOS:000263582700021 ER PT S AU Jenkins, PP Walters, RJ Krasowski, MJ Chapman, JJ Ballard, PG Vasquez, JA Mahony, DR LaCava, SN Braun, WR Skalitzky, R Prokop, NF Flatico, JM Greer, LC Gibson, KB Kinard, WH Pippin, HG AF Jenkins, Phillip P. Walters, Robert J. Krasowski, Michael J. Chapman, John J. Ballard, Perry. G. Vasquez, John A. Mahony, Denis R. LaCava, Susie N. Braun, William R. Skalitzky, Robert Prokop, Norman F. Flatico, Joseph M. Greer, Lawrence C. Gibson, Karen B. Kinard, William H. Pippin, H. Gary BE Kleiman, JI TI MISSE7: Building a Permanent Environmental Testbed for the International Space Station SO PROTECTION OF MATERIALS AND STRUCTURES FROM SPACE ENVIRONMENT SE AIP Conference Proceedings LA English DT Proceedings Paper CT 9th International Conference on Protection of Materials and Structures from Space Environment CY MAY 20-23, 2008 CL Toronto, CANADA SP Canadian Space Agcy, Montana State Univ, Univ Toronto Inst Aerospac Studies, Integr Testing Lab AB The Materials on the International Space Station Experiments (MISSE) provide low-cost material exposure experiments on the exterior of the International Space Station (ISS). The original concept for a suitcase-like box bolted to the ISS to passively expose materials to space has grown to include increasingly complex in situ characterization. As the ISS completes construction, the facilities available to MISSE experiments will increase dramatically. MISSE7 is the first MISSE to take advantage of this new infrastructure. In addition to material exposure, MISSE7 will include characterization of single-event radiation effects on electronics and solar cell performance in LEO. MISSE7 will exploit the ISS Express Logistics Carrier power and data capabilities and will leave behind a MISSE specific infrastructure for future missions. C1 [Jenkins, Phillip P.; Walters, Robert J.; Vasquez, John A.; LaCava, Susie N.; Braun, William R.; Skalitzky, Robert] USN, Res Lab, Washington, DC 20375 USA. [Krasowski, Michael J.; Prokop, Norman F.; Greer, Lawrence C.] NASA, Glenn Res Ctr, Cleveland, OH USA. [Chapman, John J.; Gibson, Karen B.; Kinard, William H.] NASA, Langley Res Ctr, Hampton, VA 23665 USA. [Ballard, Perry. G.] NASA, Johnson Space Ctr, Houston, TX USA. [Mahony, Denis R.] Praxis Inc, Alexandria, VA USA. [Flatico, Joseph M.] Ohio Aerosp Inst, Brookpark, OH USA. [Pippin, H. Gary] Boeing Phantom Works, Seattle, WA USA. RP Jenkins, PP (reprint author), USN, Res Lab, Washington, DC 20375 USA. NR 9 TC 7 Z9 7 U1 0 U2 0 PU AMER INST PHYSICS PI MELVILLE PA 2 HUNTINGTON QUADRANGLE, STE 1NO1, MELVILLE, NY 11747-4501 USA SN 0094-243X BN 978-0-7354-0619-3 J9 AIP CONF PROC PY 2009 VL 1087 BP 273 EP + PG 2 WC Engineering, Aerospace SC Engineering GA BIX44 UT WOS:000263582700023 ER PT S AU Miller, SKR Banks, BA Tollis, G AF Miller, Sharon K. R. Banks, Bruce A. Tollis, Greg BE Kleiman, JI TI MISSE Results used for RF Plasma Ground Testing-to-space-exposure Correlation for Coated Kapton SO PROTECTION OF MATERIALS AND STRUCTURES FROM SPACE ENVIRONMENT SE AIP Conference Proceedings LA English DT Proceedings Paper CT 9th International Conference on Protection of Materials and Structures from Space Environment CY MAY 20-23, 2008 CL Toronto, CANADA SP Canadian Space Agcy, Montana State Univ, Univ Toronto Inst Aerospac Studies, Integr Testing Lab AB The ability to predict the durability of materials in the low Earth orbit (LEO) environment by exposing them in ground-based facilities is important because one can achieve test results sooner, expose more types of materials, and do it much more cost effectively than to test them in flight. However, flight experiments to determine the durability of groups or classes of materials that behave similarly are needed in order to provide correlations of how much time in ground-based facilities represents certain durations in LEO for the material type of interest. An experiment was designed and flown on the Materials International Space Station Experiment (MISSE) 2 (3.95 years in LEO) and MISSE 4 (1.04 years in LEO) in order to develop this type of correlation between ground-based RF plasma exposure and LEO exposure for coated Kapton. The experiment consisted of a sample of Kapton H (R) (DuPont) polyimide coated with 1300 Angstroms of silicon dioxide by Sheldahl Inc. The samples were exposed to atomic oxygen in a radio frequency (RF) generated atomic oxygen plasma. Mass change was measured for the samples and then the same samples were exposed in flight on MISSE and the mass change was again recorded post-flight. After documentation, the samples were exposed again in the ground-based RF plasma in order to determine if the erosion would be the same as it had been in the same facility pre-flight which would indicate whether or not the sample had been damaged during flight and if the defects on the surface were those that were there pre-flight. The slopes of the mass change versus fluence plots were then used to develop a correlation factor that can be used to help predict the durability of coated Kapton in ground-based isotropic atomic oxygen plasma systems. This paper describes the experiment and presents the correlation factor results. C1 [Miller, Sharon K. R.] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. [Banks, Bruce A.] NASA, Consultant Alphaport Supporting, Washington, DC USA. [Tollis, Greg] Cleveland State Univ, Cleveland, OH 44115 USA. RP Miller, SKR (reprint author), NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. EM sharon.k.miller@nasa.gov NR 10 TC 1 Z9 1 U1 0 U2 0 PU AMER INST PHYSICS PI MELVILLE PA 2 HUNTINGTON QUADRANGLE, STE 1NO1, MELVILLE, NY 11747-4501 USA SN 0094-243X BN 978-0-7354-0619-3 J9 AIP CONF PROC PY 2009 VL 1087 BP 277 EP + PG 2 WC Engineering, Aerospace SC Engineering GA BIX44 UT WOS:000263582700024 ER PT S AU Watson, KA Ghose, S Lillehei, PT Smith, JG Connell, JW AF Watson, K. A. Ghose, S. Lillehei, P. T. Smith, J. G., Jr. Connell, J. W. BE Kleiman, JI TI Effect of LEO Exposure on Aromatic Polymers Containing Phenylphosphine Oxide Groups SO PROTECTION OF MATERIALS AND STRUCTURES FROM SPACE ENVIRONMENT SE AIP Conference Proceedings LA English DT Proceedings Paper CT 9th International Conference on Protection of Materials and Structures from Space Environment CY MAY 20-23, 2008 CL Toronto, CANADA SP Canadian Space Agcy, Montana State Univ, Univ Toronto Inst Aerospac Studies, Integr Testing Lab ID POLY(ARYLENE ETHER HETEROCYCLE)S; ATOMIC OXYGEN EXPOSURE; CONTAINING POLYIMIDES; PLASMA; FILMS; COPOLYMERS AB As part of the Materials on The International Space Station Experiment (MISSE), aromatic polymers containing phenylphosphine oxide groups were exposed to low Earth orbit for similar to 4 years. All of the aromatic polymers containing phenylphosphine oxide groups survived the exposure despite the high fluence of atomic oxygen that completely eroded other polymer films such as Kapton (R) and Mylar (R) of comparable or greater thickness. The samples were characterized for changes in physical properties, thermal/optical properties surface chemistry, and surface topography. The data from the polymer samples on MISSE were compared to samples from the same batch of material stored under ambient conditions on Earth. In addition, comparisons were made between the MISSE samples and those subjected to shorter term space flight exposures. The results of these analyses will be presented. C1 [Watson, K. A.; Ghose, S.] Natl Inst Aerosp, 100 Explorat Way, Hampton, VA 23666 USA. [Lillehei, P. T.; Smith, J. G., Jr.; Connell, J. W.] Natl Aeronaut & Space Adm, Langley Res Ctr, Hampton, VA 23681 USA. RP Watson, KA (reprint author), Natl Inst Aerosp, 100 Explorat Way, Hampton, VA 23666 USA. NR 32 TC 0 Z9 0 U1 0 U2 0 PU AMER INST PHYSICS PI MELVILLE PA 2 HUNTINGTON QUADRANGLE, STE 1NO1, MELVILLE, NY 11747-4501 USA SN 0094-243X BN 978-0-7354-0619-3 J9 AIP CONF PROC PY 2009 VL 1087 BP 291 EP + PG 3 WC Engineering, Aerospace SC Engineering GA BIX44 UT WOS:000263582700025 ER PT S AU Banks, BA de Groh, KK Miller, SK Waters, DL AF Banks, Bruce A. de Groh, Kim K. Miller, Sharon K. Waters, Deborah L. BE Kleiman, JI TI Lessons Learned from Atomic Oxygen Interaction with Spacecraft Materials in Low Earth Orbit SO PROTECTION OF MATERIALS AND STRUCTURES FROM SPACE ENVIRONMENT SE AIP Conference Proceedings LA English DT Proceedings Paper CT 9th International Conference on Protection of Materials and Structures from Space Environment CY MAY 20-23, 2008 CL Toronto, CANADA SP Canadian Space Agcy, Montana State Univ, Univ Toronto Inst Aerospac Studies, Integr Testing Lab ID RADIATION; FEP AB There have been five Materials International Space Station Experiment (MISSE) passive experiment carriers (PECs) (MISSE 1-5) to date which have been launched, exposed in space on the exterior of International Space Station (ISS) and then returned to Earth for analysis. An additional four MISSE PECs (MISSE 6A, 6B, 7A & 7B) are in various stages of completion. The PECs are two-sided suitcase size sample carriers that are intended to provide information on the effects of the low Earth orbital environment on a wide variety of materials and components. As a result of post retrieval analyses of the retrieved MISSE 2 experiments and numerous prior space experiments, there have been valuable lessons learned and needs identified that are worthy of being documented so that planning, design, and analysis of future space environment experiments can benefit from the experience in order to maximize the knowledge gained. Some of the lessons learned involve the techniques, concepts, and issues associated with measuring atomic oxygen erosion yields. These are presented along with several issues to be considered when designing experiments, such as the uncertainty in mission duration, scattering and contamination effects on results, and the accuracy of measuring atomic oxygen erosion. C1 [Banks, Bruce A.; de Groh, Kim K.; Miller, Sharon K.] NASA, Glenn Res Ctr, MS 309-2,21000 Brookpk Rd, Cleveland, OH 44135 USA. [Waters, Deborah L.] Arctic Slope Reg Corp, Barrow, AL 99723 USA. RP Banks, BA (reprint author), NASA, Glenn Res Ctr, MS 309-2,21000 Brookpk Rd, Cleveland, OH 44135 USA. EM Bruce.A.Banks@nasa.gov NR 19 TC 3 Z9 3 U1 0 U2 3 PU AMER INST PHYSICS PI MELVILLE PA 2 HUNTINGTON QUADRANGLE, STE 1NO1, MELVILLE, NY 11747-4501 USA SN 0094-243X BN 978-0-7354-0619-3 J9 AIP CONF PROC PY 2009 VL 1087 BP 312 EP + PG 4 WC Engineering, Aerospace SC Engineering GA BIX44 UT WOS:000263582700027 ER PT S AU Edwards, DL Cooke, W Suggs, R Moser, DE AF Edwards, David L. Cooke, William Suggs, Rob Moser, Danielle E. BE Kleiman, JI TI Analysis of Regolith Simulant Ejecta Distributions from Normal Incident Hypervelocity Impact SO PROTECTION OF MATERIALS AND STRUCTURES FROM SPACE ENVIRONMENT SE AIP Conference Proceedings LA English DT Proceedings Paper CT 9th International Conference on Protection of Materials and Structures from Space Environment CY MAY 20-23, 2008 CL Toronto, CANADA SP Canadian Space Agcy, Montana State Univ, Univ Toronto Inst Aerospac Studies, Integr Testing Lab AB The National Aeronautics and Space Administration (NASA) has established the Constellation Program. The Constellation Program has defined one of its many goals as long-term lunar habitation. Critical to the design of a lunar habitat is an understanding of the lunar surface environment; of specific importance is the primary meteoroid and subsequent ejecta environment. The document, NASA SP-8013 "Meteoroid Environment Model Near Earth to Lunar Surface", was developed for the Apollo program in 1969 and contains the latest definition of the lunar ejecta environment. There is concern that NASA SP-8013 may overestimate the lunar ejecta environment. NASA's Meteoroid Environment Office (MEO) has initiated several tasks to improve the accuracy of our understanding of the lunar surface ejecta environment. This paper reports the results of experiments on projectile impact into powdered pumice and unconsolidated JSC-1A Lunar Mare Regolith simulant targets. Projectiles were accelerated to velocities between 2.45 and 5.18 km/s and impacted the targets at normal incidence using the Ames Vertical Gun Range (AVGR). The ejected particles were detected by thin aluminum foil targets strategically placed around the impact site and angular ejecta distributions were determined. Assumptions were made to support the analysis which include; assuming ejecta spherical symmetry resulting from normal impact and all ejecta particles were of mean target particle size. This analysis produces a hemispherical flux density distribution of ejecta with sufficient velocity to penetrate the aluminum foil detectors. C1 [Edwards, David L.; Cooke, William; Suggs, Rob] NASA, George C Marshall Space Flight Ctr, M-S EV44 MSFC, Huntsville, AL 35812 USA. RP Edwards, DL (reprint author), NASA, George C Marshall Space Flight Ctr, M-S EV44 MSFC, Huntsville, AL 35812 USA. NR 4 TC 0 Z9 0 U1 0 U2 1 PU AMER INST PHYSICS PI MELVILLE PA 2 HUNTINGTON QUADRANGLE, STE 1NO1, MELVILLE, NY 11747-4501 USA SN 0094-243X BN 978-0-7354-0619-3 J9 AIP CONF PROC PY 2009 VL 1087 BP 559 EP + PG 2 WC Engineering, Aerospace SC Engineering GA BIX44 UT WOS:000263582700050 ER PT S AU Kleiman, JI Iskanderova, Z Issoupov, V Grigorevskiy, AV Kiseleva, LV Finckenor, M Naumov, SF Sokolova, SP Kurilenok, AO AF Kleiman, J. I. Iskanderova, Z. Issoupov, V. Grigorevskiy, A. V. Kiseleva, L. V. Finckenor, M. Naumov, S. F. Sokolova, S. P. Kurilenok, A. O. BE Kleiman, JI TI The Results of Ground-based and In-flight Testing of Charge-dissipative and Conducting EKOM Thermal Control Paints SO PROTECTION OF MATERIALS AND STRUCTURES FROM SPACE ENVIRONMENT SE AIP Conference Proceedings LA English DT Proceedings Paper CT 9th International Conference on Protection of Materials and Structures from Space Environment CY MAY 20-23, 2008 CL Toronto, CANADA SP Canadian Space Agcy, Montana State Univ, Univ Toronto Inst Aerospac Studies, Integr Testing Lab ID SURFACE MODIFICATION; SPACE DURABILITY; ENHANCEMENT AB An international program on comparative evaluation of space durability of thermal control paints from a number of countries was initiated a few years ago at ITL with coatings from Russia, France and USA being studied. This paper describes the results of the study on space durability of three types of charge-dissipative and conductive Russian advanced polymer-based EKOM thermal control paints. Extensive ground-based testing in fast atomic oxygen (FAO) beam facilities was used to test the space durability of these paints and the enhancement of their atomic oxygen erosion resistance by a surface modification technology, Photosil (TM). All pristine EKOM paints were also tested in a direct materials exposure experiment on Russian module "Zvezda" onboard the International Space Station. Space durability and change of the major physical properties were evaluated after these experiments using a number of analytical techniques. Both, the ground-based testing and the flight experiments indicated signs of surface erosion with some changes of thermal optical properties. Therefore, the paints were also modified by a surface treatment technology, Photosil (TM), to increase their erosion resistance to atomic oxygen, tested in the same ground-based FAO facilities up to high FAO fluencies and compared with testing results of pristine materials. The comparison indicated that the surface-modified paints exhibit reduced mass loss, full stabilization and no surface morphology changes, thus indicating at full protection from the high FAO fluencies. It was demonstrated that the developed surface modification treatment could be applied successfully to charge dissipative and conductive paints, to enhance the low Earth orbit (LEO) environment resistance of external thermal control coatings in long-term space missions. C1 [Kleiman, J. I.; Iskanderova, Z.; Issoupov, V.] Integr Testing Lab Inc, Markham, ON, Canada. [Grigorevskiy, A. V.; Kiseleva, L. V.] JSC Kompozit Korolev, Moscow, Russia. [Finckenor, M.] NASA, Marshall Space Fight Ctr, Huntsville, AL 35811 USA. [Naumov, S. F.; Sokolova, S. P.; Kurilenok, A. O.] RSC Energia Korolev, Moscow, Russia. RP Kleiman, JI (reprint author), Integr Testing Lab Inc, Markham, ON, Canada. EM ziskanderova@itlinc.com NR 10 TC 0 Z9 0 U1 0 U2 1 PU AMER INST PHYSICS PI MELVILLE PA 2 HUNTINGTON QUADRANGLE, STE 1NO1, MELVILLE, NY 11747-4501 USA SN 0094-243X BN 978-0-7354-0619-3 J9 AIP CONF PROC PY 2009 VL 1087 BP 610 EP + PG 3 WC Engineering, Aerospace SC Engineering GA BIX44 UT WOS:000263582700056 ER PT S AU Hays, CC Kulleck, JG Haines, BE Narayan, SR AF Hays, C. C. Kulleck, J. G. Haines, B. E. Narayan, S. R. BE Fuller, T Uchida, H Strasser, P Shirvanian, P Lamy, C Hartnig, C Gasteiger, HA Zawodzinski, T Jarvi, T Bele, P Ramani, V Cleghorn, S Jones, D Zelenay, P TI Thin Film Platinum Alloys For Use As Catalyst Materials In Fuel Cells SO PROTON EXCHANGE MEMBRANE FUEL CELLS 9 SE ECS Transactions LA English DT Proceedings Paper CT 9th Proton Exchange Membrane Fuel Cell Symposium (PEMFC) Conducted Under the Auspices of the 216th Meeting of the Electrochemical-Society-Inc CY OCT 04-09, 2009 CL Vienna, AUSTRIA SP Electrochem Soc Inc, Electrochem Soc, Energy Technol Div, Electrochem Soc, Ind Electrochemistry & Electrochem Engn, Electrochem Soc, Phys & Analyt Electrochemistry Div, Electrochem Soc, Battery Div, Automot Fuel Cell Cooperat Corp, Ion Power, N E Chemcat Corp, Pine Res Instrumentat Inc, Tanaka Kikinzoku Kogyo, Toyota Motor Engn & Mfg Amer, Tokuyama Corp, Umicore AG & Co KG, UTC Power Corp AB Measurements of the structural and electrochemical properties of nanostructured thin film alloys in the ternary series Pt-Co-Zr are presented. These alloys have been studied to determine the influence of early transition metal element additions on the catalytic response and chemical stability of platinum-group-metal (PGM) alloys in acid electrolytes. The thin film compositions in the Pt-Co-Zr system were prepared via co-sputtering and the films exhibit a (111) crystallographic orientation. Alloys with Pt-metal contents of less than 50 At. % are stable in 0.1 M perchloric acid electrolytes, and are electrochemically active for the oxygen reduction reaction (ORR). The ORR kinetic currents at 0.9 V are comparable to Pt. The alloys have been cycled over the range 0.0 to 1.2 V NHE, with no degradation of the electrode surface area or decrease in electrochemical performance observed. Our results suggest that Pt-Co-Zr alloys with reduced PGM contents may be competitive with Pt-catalysts. C1 [Hays, C. C.; Kulleck, J. G.; Haines, B. E.; Narayan, S. R.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Hays, CC (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. NR 2 TC 0 Z9 0 U1 0 U2 3 PU ELECTROCHEMICAL SOC INC PI PENNINGTON PA 65 S MAIN ST, PENNINGTON, NJ 08534-2839 USA SN 1938-5862 BN 978-1-60768-088-8 J9 ECS TRANSACTIONS PY 2009 VL 25 IS 1 BP 619 EP 623 DI 10.1149/1.3210613 PG 5 WC Electrochemistry; Energy & Fuels SC Electrochemistry; Energy & Fuels GA BJQ12 UT WOS:000329585500060 ER PT S AU Valdez, TI Billings, KJ Sakamoto, J Mansfeld, F Narayanan, SR AF Valdez, Thomas I. Billings, Keith J. Sakamoto, Jeff Mansfeld, Florian Narayanan, S. R. BE Fuller, T Uchida, H Strasser, P Shirvanian, P Lamy, C Hartnig, C Gasteiger, HA Zawodzinski, T Jarvi, T Bele, P Ramani, V Cleghorn, S Jones, D Zelenay, P TI Iridium and Lead Doped Ruthenium Oxide Catalysts for Oxygen Evolution SO PROTON EXCHANGE MEMBRANE FUEL CELLS 9 SE ECS Transactions LA English DT Proceedings Paper CT 9th Proton Exchange Membrane Fuel Cell Symposium (PEMFC) Conducted Under the Auspices of the 216th Meeting of the Electrochemical-Society-Inc CY OCT 04-09, 2009 CL Vienna, AUSTRIA SP Electrochem Soc Inc, Electrochem Soc, Energy Technol Div, Electrochem Soc, Ind Electrochemistry & Electrochem Engn Div, Electrochem Soc, Phys & Analyt Electrochemistry Div, Electrochem Soc, Battery Div, Automot Fuel Cell Cooperat Corp, Ion Power, N E Chemcat Corp, Pine Res Instrumentat Inc, Tanaka Kikinzoku Kogyo, Toyota Motor Engn & Mfg Amer, Tokuyama Corp, Umicore AG & Co KG, UTC Power Corp ID SOLID POLYMER ELECTROLYTE; WATER ELECTROLYSIS; ANODIC EVOLUTION; ELECTROCATALYSIS; SURFACES AB The performance of various ruthenium oxide-based oxygen evolution catalysts fabricated by various techniques has been studied. A thermal processing technique has been identified that can produce stable iridium and lead-doped ruthenium oxide catalysts. The best performance for the oxygen evolution reaction was obtained with iridium-doped ruthenium oxide catalyst containing nine-mole percent iridium. The cell voltage of the Ir(9%)-d-RuO2 catalyst at an applied current density of 200-mA/cm(2) was 1.45 Volts at 70 degrees C. The oxygen evolution Tafel slopes for the doped ruthenium oxide catalysts were in the range of 40 to 55-mV/decade. C1 [Valdez, Thomas I.; Billings, Keith J.; Sakamoto, Jeff; Narayanan, S. R.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. [Mansfeld, Florian] Univ So Calif, Los Angeles, CA 90089 USA. RP Valdez, TI (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. NR 15 TC 7 Z9 7 U1 0 U2 1 PU ELECTROCHEMICAL SOC INC PI PENNINGTON PA 65 S MAIN ST, PENNINGTON, NJ 08534-2839 USA SN 1938-5862 BN 978-1-60768-088-8 J9 ECS TRANSACTIONS PY 2009 VL 25 IS 1 BP 1371 EP 1382 DI 10.1149/1.3210693 PG 12 WC Electrochemistry; Energy & Fuels SC Electrochemistry; Energy & Fuels GA BJQ12 UT WOS:000329585500140 ER PT J AU Petrov, L Phillips, C Bertarini, A Deller, A Pogrebenko, S Mujunen, A AF Petrov, Leonid Phillips, Chris Bertarini, Alessandra Deller, Adam Pogrebenko, Sergei Mujunen, Ari TI Use of the Long Baseline Array in Australia for Precise Geodesy and Absolute Astrometry SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF AUSTRALIA LA English DT Article DE instrumentation: interferometers; techniques: interferometric; reference systems ID VLBA CALIBRATOR SURVEY; HIGHER RADIO FREQUENCIES; INTERFEROMETRY; ICRF; TITAN AB We report the results of a successful 12-hour 22-GHz VLBI experiment using a heterogeneous network that includes radio telescopes of the Long Baseline Array (LBA) in Australia and several VLBI stations that regularly observe in geodetic VLBI campaigns. We have determined positions of three VLBI stations, ATCA-104, CEDUNA and MOPRA, with an accuracy of 4-30 mm using a novel technique of data analysis. These stations have never before participated in geodetic experiments. We observed 105 radio sources, and amongst them 5 objects which have not previously been observed with VLBI. We have determined positions of these new sources with the accuracy of 2-5 mas. We make the conclusion that the LBA network is capable of conducting absolute astrometry VLBI surveys with an accuracy better than 5 mas. C1 [Petrov, Leonid] NASA, Goddard Space Flight Ctr, ADNET Syst Inc, Greenbelt, MD 20771 USA. [Bertarini, Alessandra] Inst Geodesy & Geoinformat, Bonn, Germany. [Deller, Adam] Swinburne Univ Technol, Ctr Astrophys & Supercomp, Hawthorn, Vic 3123, Australia. [Mujunen, Ari] Helsinki Univ Technol, TKK, Metsahovi Radio Observ, FIN-02150 Espoo, Finland. RP Petrov, L (reprint author), NASA, Goddard Space Flight Ctr, ADNET Syst Inc, Code 610-2, Greenbelt, MD 20771 USA. EM Leonid.Petrov@lpetrov.net OI Deller, Adam/0000-0001-9434-3837 FU European Commission [026642] FX EXPReS is an Integrated Infrastructure Initiative (I3), funded under the European Commission's Sixth Framework Programme (FP6), contract number 026642, from March 2006 through February 2009. We greatly appreciate Alan Fey and Roopesh Ojha who made digital images in FITS format from the surveys publicly available and Robert Campbell for performing the highly non-standard test correlations of LBA data at the JIVE correlator. NR 31 TC 5 Z9 5 U1 0 U2 1 PU CSIRO PUBLISHING PI COLLINGWOOD PA 150 OXFORD ST, PO BOX 1139, COLLINGWOOD, VICTORIA 3066, AUSTRALIA SN 1323-3580 J9 PUBL ASTRON SOC AUST JI Publ. Astron. Soc. Aust. PY 2009 VL 26 IS 1 BP 75 EP 84 DI 10.1071/AS08030 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 427EI UT WOS:000264762200009 ER PT J AU Shaddock, DA AF Shaddock, D. A. TI An Overview of the Laser Interferometer Space Antenna SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF AUSTRALIA LA English DT Article DE gravitational waves; techniques: interferometric ID FREQUENCY STABILIZATION; LISA ARM; LOCKING; DELAY AB The Laser Interferometer Space Antenna (LISA) will detect gravitational waves with frequencies from 0.1 mHz to 1 Hz. This article provides a brief overview of LISA's science goals followed by a tutorial of the LISA measurement concept. C1 [Shaddock, D. A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Shaddock, D. A.] Australian Natl Univ, Ctr Gravitat Phys, Canberra, ACT 0200, Australia. RP Shaddock, DA (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM daniel.shaddock@jpl.nasa.gov RI Shaddock, Daniel/A-7534-2011 OI Shaddock, Daniel/0000-0002-6885-3494 FU Australian Research Council [DP0666437] FX I would like to thank the Astronomical Society of Australia for the invitation to submit this paper as a result of an invited talk at the ASM. The work reported on here is a summary of the work of the LISA community and I gratefully acknowledge the hard work of many researchers around the world. Parts of this research were performed at the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. This research was also supported by the Australian Research Council's Discovery Projects funding scheme (project number DP0666437). NR 27 TC 7 Z9 7 U1 0 U2 2 PU CSIRO PUBLISHING PI COLLINGWOOD PA 150 OXFORD ST, PO BOX 1139, COLLINGWOOD, VICTORIA 3066, AUSTRALIA SN 1323-3580 J9 PUBL ASTRON SOC AUST JI Publ. Astron. Soc. Aust. PY 2009 VL 26 IS 2 BP 128 EP 132 DI 10.1071/AS08059 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 462MS UT WOS:000267358100004 ER PT J AU Sterling, NC Dinerstein, HL Hwang, S Redfield, S Aguilar, A Witthoeft, MC Esteves, D Kilcoyne, ALD Bautista, M Phaneuf, R Bilodeau, RC Ballance, CP McLaughlin, B Norrington, PH AF Sterling, N. C. Dinerstein, H. L. Hwang, S. Redfield, S. Aguilar, A. Witthoeft, M. C. Esteves, D. Kilcoyne, A. L. D. Bautista, M. Phaneuf, R. Bilodeau, R. C. Ballance, C. P. McLaughlin, B. Norrington, P. H. TI Improved Neutron-Capture Element Abundances in Planetary Nebulae SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF AUSTRALIA LA English DT Article DE planetary nebulae: general; nuclear reactions, nucleosynthesis, abundances; stars: AGB and post-AGB; atomic data ID ASYMPTOTIC GIANT BRANCH; S-PROCESS ABUNDANCES; R-MATRIX METHOD; CHEMICAL-COMPOSITION; ELECTRON-SCATTERING; STARS; NUCLEOSYNTHESIS; IDENTIFICATION; NGC-7027; KRYPTON AB Spectroscopy of planetary nebulae (PNe) provides the means to investigate s-process enrichments of neutron(n)-capture elements that cannot be detected in Asymptotic Giant Branch (AGB) stars. However, accurate abundance determinations of these elements present a challenge. Corrections for unobserved ions can be large and uncertain, since in many PNe only one ion of a given n-capture element has been detected. Furthermore, the atomic data governing the ionization balance of these species are not well-determined, inhibiting the derivation of accurate ionization corrections. We present initial results of a program that addresses these challenges. Deep high-resolution optical spectroscopy of similar to 20 PNe has been performed to detect emission lines from trans-iron species including Se, Br, Kr, Rb and Xe. The optical spectral region provides access to multiple ions of these elements, which reduces the magnitude and importance of uncertainties in the ionization corrections. In addition, experimental and theoretical efforts are providing determinations of the photoionization cross sections and recombination rate coefficients of Se, Kr and Xe ions. These new atomic data will make it possible to derive robust ionization corrections for these elements. Together, our observational and atomic data results will enable n-capture element abundances to be determined with unprecedented accuracy in ionized nebulae. C1 [Sterling, N. C.; Witthoeft, M. C.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Dinerstein, H. L.; Hwang, S.] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA. [Redfield, S.] Wesleyan Univ, Dept Astron, Van Vleck Observ, Middletown, CT 06459 USA. [Aguilar, A.; Kilcoyne, A. L. D.; Bilodeau, R. C.] Univ Calif Berkeley, Lawrence Berkeley Lab, Adv Light Source, Berkeley, CA 94270 USA. [Esteves, D.; Phaneuf, R.] Univ Nevada, Dept Phys, Reno, NV 89557 USA. [Bautista, M.] Virginia Polytech Inst & State Univ, Dept Phys, Blacksburg, VA 24061 USA. [Ballance, C. P.] Auburn Univ, Dept Phys, Auburn, AL USA. [McLaughlin, B.; Norrington, P. H.] Queens Univ Belfast, Sch Math & Phys, Ctr Atom Mol & Opt Phys, Belfast BT7 1NN, Antrim, North Ireland. RP Sterling, NC (reprint author), NASA, Goddard Space Flight Ctr, Code 662, Greenbelt, MD 20771 USA. EM nicholas.c.sterling@nasa.gov RI Kilcoyne, David/I-1465-2013; OI Bilodeau, Rene/0000-0001-8607-2328; Redfield, Seth/0000-0003-3786-3486 FU US National Science Foundation [AST 0708245, 0406809]; US DOE [DE-FG02-05R54819, DE-FG02-99ER54367]; NASA [06-APRA206-0049] FX We gratefully acknowledge J. Bizau, who sent us experimental PI cross section data for Xe3+ through Xe6+. N.C.S. is supported by an appointment to the NASA Post-doctoral Program, administered by Oak Ridge Associated Universities through a contract with NASA. B. M. M. acknowledges support by the US National Science Foundation through a grant to ITAMP at the Harvard-Smithsonian Center for Astrophysics. C. P. B. is supported by US DOE grants DE-FG02-05R54819 and DE-FG02-99ER54367. The DARC computations were conducted at the National Energy Research Scientific Computing Center in Oakland, CA. This work has been partially supported by NASA grant 06-APRA206-0049 and NSF grants AST 0708245 and 0406809. NR 31 TC 19 Z9 19 U1 0 U2 2 PU CSIRO PUBLISHING PI COLLINGWOOD PA 150 OXFORD ST, PO BOX 1139, COLLINGWOOD, VICTORIA 3066, AUSTRALIA SN 1323-3580 J9 PUBL ASTRON SOC AUST JI Publ. Astron. Soc. Aust. PY 2009 VL 26 IS 3 BP 339 EP 344 DI 10.1071/AS08067 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 498ID UT WOS:000270131300035 ER PT J AU Lawrence, JS Ashley, MCB Bailey, J Navascues, DBY Bedding, TR Bland-Hawthorn, J Bond, I Boulanger, F Bouwens, R Bruntt, H Bunker, A Burgarella, D Burton, MG Busso, M Coward, D Cioni, MR Durand, G Eiroa, C Epchtein, N Gehrels, N Gillingham, P Glazebrook, K Haynes, R Kiss, L Lagage, PO Le Bertre, T Mackay, C Maillard, JP McGrath, A Minier, V Mora, A Olsen, K Persi, P Pimbblet, K Quimby, R Saunders, W Schmidt, B Stello, D Storey, JWV Tinney, C Tremblin, P Wheeler, JC Yock, P AF Lawrence, J. S. Ashley, M. C. B. Bailey, J. Barrado y Navascues, D. Bedding, T. R. Bland-Hawthorn, J. Bond, I. Boulanger, F. Bouwens, R. Bruntt, H. Bunker, A. Burgarella, D. Burton, M. G. Busso, M. Coward, D. Cioni, M. -R. Durand, G. Eiroa, C. Epchtein, N. Gehrels, N. Gillingham, P. Glazebrook, K. Haynes, R. Kiss, L. Lagage, P. O. Le Bertre, T. Mackay, C. Maillard, J. P. McGrath, A. Minier, V. Mora, A. Olsen, K. Persi, P. Pimbblet, K. Quimby, R. Saunders, W. Schmidt, B. Stello, D. Storey, J. W. V. Tinney, C. Tremblin, P. Wheeler, J. C. Yock, P. TI The Science Case for PILOT I: Summary and Overview SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF AUSTRALIA LA English DT Editorial Material DE cosmology: observations; early universe; instrumentation: high angular resolution; site testing; stars: formation; telescopes ID INFRARED SKY BRIGHTNESS; SPITZER-SPACE-TELESCOPE; HIGH-ANTARCTIC PLATEAU; DOME-C; SOUTH-POLE; RADIO OBSERVATIONS; ASTRONOMY; ARRAY; TURBULENCE; UNIVERSE AB PILOT (the Pathfinder for an International Large Optical Telescope) is a proposed 2.5-m optical/infrared telescope to be located at Dome C on the Antarctic plateau. Conditions at Dome C are known to be exceptional for astronomy. The seeing (above similar to 30m height), coherence time, and isoplanatic angle are all twice as good as at typical mid-latitude sites, while the water-vapour column, and the atmosphere and telescope thermal emission are all an order of magnitude better. These conditions enable a unique scientific capability for PILOT, which is addressed in this series of papers. The current paper presents an overview of the optical and instrumentation suite for PILOT and its expected performance, a summary of the key science goals and observational approach for the facility, a discussion of the synergies between the science goals for PILOT and other telescopes, and a discussion of the future of Antarctic astronomy. Paper II and Paper III present details of the science projects divided, respectively, between the distant Universe (i.e. studies of first light, and the assembly and evolution of structure) and the nearby Universe (i.e. studies of Local Group galaxies, the Milky Way, and the Solar System). C1 [Lawrence, J. S.; Ashley, M. C. B.; Bailey, J.; Burton, M. G.; Storey, J. W. V.; Tinney, C.] Univ New S Wales, Sch Phys, Sydney, NSW 2052, Australia. [Barrado y Navascues, D.] Lab Astrofis Espacial & Fis Fundamental INTA, Madrid 28080, Spain. [Bedding, T. R.; Bland-Hawthorn, J.; Bruntt, H.; Kiss, L.; Stello, D.] Univ Sydney, Sch Phys, Inst Astron, Sydney, NSW 2006, Australia. [Bond, I.] Massey Univ, Auckland 0745, New Zealand. [Boulanger, F.] Univ Paris 11, Inst Astrophys Spatiale, F-91405 Orsay, France. [Bouwens, R.] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA. [Bunker, A.; Gillingham, P.; Haynes, R.; McGrath, A.; Saunders, W.] Anglo Australian Observ, Epping, NSW 1710, Australia. [Busso, M.] Univ Perugia, Dept Phys, I-06123 Perugia, Italy. [Burgarella, D.] Univ Aix Marseille, Observ Astron Marseille Provence, F-13388 Marseille, France. [Coward, D.] Univ Western Australia, Sch Phys, Crawley, WA 6009, Australia. [Cioni, M. -R.] Univ Hertfordshire, Ctr Astrophys Res, Hatfield AL10 9AB, Herts, England. [Durand, G.; Lagage, P. O.; Minier, V.; Tremblin, P.] CEA Saclay, Serv Astrophys, F-91191 Saclay, France. [Eiroa, C.; Mora, A.] Univ Autonoma Madrid, Dept Fis Teor C 11, E-28049 Madrid, Spain. [Epchtein, N.] UNSA, CNRS Fizeau, F-06108 Nice, France. [Gehrels, N.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Glazebrook, K.] Swinburne Univ Technol, Ctr Astrophys & Supercomp, Hawthorn, Vic 3122, Australia. [Le Bertre, T.] Observ Paris, F-75014 Paris, France. [Mackay, C.] Univ Cambridge, Inst Astron, Cambridge CB3 0HE, England. [Maillard, J. P.] Inst Astrophys, F-75014 Paris, France. [Olsen, K.] Natl Opt Astron Observ, Kitt Peak Natl Observ, Tucson, AZ 85719 USA. [Persi, P.] Ist Astrofis Spaziale & Fis Cosm INAF, I-00100 Rome, Italy. [Pimbblet, K.] Univ Queensland, Dept Phys, Brisbane, Qld 4072, Australia. [Quimby, R.] CALTECH, Dept Astron, Pasadena, CA 91125 USA. [Schmidt, B.] Australian Natl Univ, Res Sch Astron & Astrophys, Weston, ACT 2611, Australia. [Wheeler, J. C.] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA. [Yock, P.] Univ Auckland, Auckland 1142, New Zealand. RP Lawrence, JS (reprint author), Macquarie Univ, Dept Phys & Engn, N Ryde, NSW 2109, Australia. EM jsl@science.mq.edu.au RI Gehrels, Neil/D-2971-2012; Glazebrook, Karl/N-3488-2015; Barrado Navascues, David/C-1439-2017; Busso, Maurizio Maria/K-7075-2015; OI Glazebrook, Karl/0000-0002-3254-9044; Barrado Navascues, David/0000-0002-5971-9242; Busso, Maurizio Maria/0000-0001-8944-5820; Burton, Michael/0000-0001-7289-1998; Schmidt, Brian/0000-0001-6589-1287; Tremblin, Pascal/0000-0001-6172-3403; Tinney, Christopher/0000-0002-7595-0970 NR 82 TC 10 Z9 11 U1 0 U2 4 PU CAMBRIDGE UNIV PRESS PI NEW YORK PA 32 AVENUE OF THE AMERICAS, NEW YORK, NY 10013-2473 USA SN 1323-3580 EI 1448-6083 J9 PUBL ASTRON SOC AUST JI Publ. Astron. Soc. Aust. PY 2009 VL 26 IS 4 BP 379 EP 396 DI 10.1071/AS08048 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 514SM UT WOS:000271415900001 ER PT J AU Lawrence, JS Ashley, MCB Bunker, A Bouwens, R Burgarella, D Burton, MG Gehrels, N Glazebrook, K Pimbblet, K Quimby, R Saunders, W Storey, JWV Wheeler, JC AF Lawrence, J. S. Ashley, M. C. B. Bunker, A. Bouwens, R. Burgarella, D. Burton, M. G. Gehrels, N. Glazebrook, K. Pimbblet, K. Quimby, R. Saunders, W. Storey, J. W. V. Wheeler, J. C. TI The Science Case for PILOT II: the Distant Universe SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF AUSTRALIA LA English DT Review DE early universe; cosmology: observations; galaxies: clusters: general; galaxies: high-redshift; large-scale structure of universe; supernovae: general; telescopes ID GAMMA-RAY BURST; COLOR-DENSITY RELATION; HIGH-REDSHIFT UNIVERSE; GALAXY STAR-FORMATION; DOME-C; MASSIVE GALAXIES; POPULATION-III; IA SUPERNOVAE; 1ST STARS; ENVIRONMENTAL DEPENDENCE AB PILOT (the Pathfinder for an International Large Optical Telescope) is a proposed 2.5-m optical/infrared telescope to be located at Dome C on the Antarctic plateau. The atmospheric conditions at Dome C deliver a high sensitivity, high photometric precision, wide-field, high spatial resolution, and high-cadence imaging capability to the PILOT telescope. These capabilities enable a unique scientific potential for PILOT, which is addressed in this series of papers. The current paper presents a series of projects dealing with the distant (redshift > 1) Universe, that have been identified as key science drivers for the PILOT facility. The potential for PILOT to detect the first populations of stars to form in the early Universe, via infrared projects searching for pair-instability supernovae and gamma-ray burst afterglows, is investigated. Two projects are proposed to examine the assembly and evolution of structure in the Universe: an infrared survey searching for the first evolved galaxies at high redshift, and an optical survey aimed at characterising moderate-redshift galaxy clusters. Finally, a large-area weak-lensing survey and a program to obtain supernova infrared light-curves are proposed to examine the nature and evolution of dark energy and dark matter. C1 [Lawrence, J. S.; Ashley, M. C. B.; Burton, M. G.; Storey, J. W. V.] Univ New S Wales, Sch Phys, Sydney, NSW 2052, Australia. [Bunker, A.; Saunders, W.] Anglo Australian Observ, Epping, NSW 1710, Australia. [Bouwens, R.] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA. [Burgarella, D.] Univ Aix Marseille, Observ Astron Marseille Provence, F-13388 Marseille, France. [Gehrels, N.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Glazebrook, K.] Swinburne Univ Technol, Ctr Astrophys & Supercomp, Hawthorn, Vic 3122, Australia. [Pimbblet, K.] Univ Queensland, Dept Phys, Brisbane, Qld 4072, Australia. [Quimby, R.] CALTECH, Dept Astron, Pasadena, CA 91125 USA. [Wheeler, J. C.] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA. RP Lawrence, JS (reprint author), Macquarie Univ, Dept Phys & Engn, N Ryde, NSW 2109, Australia. EM jsl@science.mq.edu.au RI Gehrels, Neil/D-2971-2012; Glazebrook, Karl/N-3488-2015; OI Glazebrook, Karl/0000-0002-3254-9044; Burton, Michael/0000-0001-7289-1998 FU Australian Department of Education, Science, and Training through the National Collaborative Research Infrastructure Strategy (NCRIS); University of New South Wales through the UNSW PILOT Science Office; European Commission [RICA26150] FX The PILOT Science Case, presented here, was produced as part of the PILOT conceptual design study, funded through the Australian Department of Education, Science, and Training through the National Collaborative Research Infrastructure Strategy (NCRIS) scheme, and the University of New South Wales through the UNSW PILOT Science Office. The European contribution has been supported by the ARENA network of the European Commission FP6 under contract RICA26150. NR 106 TC 6 Z9 7 U1 0 U2 1 PU CSIRO PUBLISHING PI COLLINGWOOD PA 150 OXFORD ST, PO BOX 1139, COLLINGWOOD, VICTORIA 3066, AUSTRALIA SN 1323-3580 J9 PUBL ASTRON SOC AUST JI Publ. Astron. Soc. Aust. PY 2009 VL 26 IS 4 BP 397 EP 414 DI 10.1071/AS08049 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 514SM UT WOS:000271415900002 ER PT J AU Shao, M Nemati, B AF Shao, M. Nemati, B. TI Sub-Microarcsecond Astrometry with SIM-Lite: A Testbed-based Performance Assessment SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF THE PACIFIC LA English DT Article AB SIM-Lite is an astrometric interferometer being designed for sub-microarcsecond astrometry, with a wide range of applications from searches for Earth-analogs to determining the distribution of dark matter. SIM-Lite measurements can be limited by random and systematic errors, as well as astrophysical noise. In this paper we focus on instrument systematic errors and report results from SIM-Lite's interferometer testbed. We find that, for narrow-angle astrometry such as used for planet finding, the end-of-mission noise floor for SIM-Lite is below 0.035 mu as. C1 [Shao, M.; Nemati, B.] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. RP Shao, M (reprint author), CALTECH, Jet Prop Lab, MS 301-486, Pasadena, CA 91125 USA. FU Copyright 2008 California Institute of Technology FX The research described in this article was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. Copyright 2008 California Institute of Technology. Government sponsorship acknowledged. NR 10 TC 9 Z9 9 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-6280 J9 PUBL ASTRON SOC PAC JI Publ. Astron. Soc. Pac. PD JAN PY 2009 VL 121 IS 875 BP 41 EP 44 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 404LF UT WOS:000263152600005 ER PT J AU Myhre, G Berglen, TF Hoyle, CR Christopher, SA Coe, H Crosier, J Formenti, P Haywood, JM Johnsrud, M Jones, TA Loeb, N Osborne, S Remer, LA AF Myhre, G. Berglen, T. F. Hoyle, C. R. Christopher, S. A. Coe, H. Crosier, J. Formenti, P. Haywood, J. M. Johnsrud, M. Jones, T. A. Loeb, N. Osborne, S. Remer, L. A. TI Modelling of chemical and physical aerosol properties during the ADRIEX aerosol campaign SO QUARTERLY JOURNAL OF THE ROYAL METEOROLOGICAL SOCIETY LA English DT Article DE aircraft measurements; secondary organic aerosols; radiative forcing ID SECONDARY ORGANIC AEROSOL; INDIAN-OCEAN EXPERIMENT; DUST EXPERIMENT SHADE; RADIATIVE IMPACT; OPTICAL-PROPERTIES; TRANSPORT MODEL; GLOBAL AEROSOL; AIR-POLLUTION; OSLO CTM2; SEA-SALT AB A global aerosol model with relatively high resolution is used to simulate the distribution and radiative effect of aerosols during the Aerosol Direct Radiative Impact Experiment (ADRIEX) campaign in August and September 2004. The global chemical transport model Oslo CTM2 includes detailed chemistry, which is coupled to aerosol partitioning of sulphate, nitrate and secondary organic aerosols. In accordance with aircraft observations the aerosol model simulates a dominance of secondary aerosols compared to primary aerosols in the ADRIEX study region. The model underestimates the aerosol optical depth (AOD) at 550 nm in the main region of the campaign around Venice. This underestimation mainly occurs during a 3-4 day period of highest AODs. At two AERONET (Aerosol Robotic Network) stations related to the ADRIEX campaign outside the Po valley area, the model compares very well with the observed AOD. Comparisons with observed chemical composition show that the model mainly underestimates organic carbon, with better agreement for other aerosol species. The model simulations indicate that the emission of aerosols and their precursors may be underestimated in the Po valley. Recent results show a large spread in radiative forcing due to the direct aerosol effect in global aerosol models, which is likely linked to large. differences in the vertical profile of aerosols and aerosol absorption. The modelled vertical profile of aerosol compares reasonably well to the aircraft measurements as was the case in two earlier campaigns involving biomass burning and dust aerosols. The radiative effect of aerosols over the northern part of the Adriatic Sea agrees well with the mean of three satellite-derived estimates despite large differences between the satellite-derived data. The difference between the model and the mean of the satellite data is within 10% for the radiative effect. The radiative forcing due to anthropogenic aerosols is simulated to be negative in the ADRIEX region with values between -5 and -2 W m(-2). Copyright (C) 2008 Royal Meteorological Society and Crown Copyright C1 [Myhre, G.; Berglen, T. F.; Hoyle, C. R.] Univ Oslo, Dept Geosci, N-0315 Oslo, Norway. [Myhre, G.] Ctr Int Climate & Environm Res, Oslo, Norway. [Christopher, S. A.; Jones, T. A.] Univ Alabama, Dept Atmospher Sci, Huntsville, AL 35899 USA. [Coe, H.; Crosier, J.] Univ Manchester, Manchester M13 9PL, Lancs, England. [Formenti, P.] Univ Paris 12, LISA, Creteil, France. [Formenti, P.] Univ Paris 07, LISA, Creteil, France. [Haywood, J. M.; Osborne, S.] Met Off, Exeter, Devon, England. [Johnsrud, M.] Norwegian Inst Air Res NILU, Kjeller, Norway. [Loeb, N.] NASA, Langley Atmospher Res Ctr LaRC, Hampton, VA USA. [Remer, L. A.] NASA, Goddard Space Flight Ctr, Atmospheres Lab, Greenbelt, MD 20771 USA. RP Myhre, G (reprint author), Univ Oslo, Dept Geosci, POB 1022, N-0315 Oslo, Norway. EM gunnar.myhre@geo.uio.no RI Myhre, Gunnar/A-3598-2008; Crosier, Jonathan/G-8952-2011; Christopher, Sundar/E-6781-2011; Coe, Hugh/C-8733-2013; Hoyle, Christopher/B-7786-2008; OI Myhre, Gunnar/0000-0002-4309-476X; Hoyle, Christopher/0000-0002-1369-9143; Crosier, Jonathan/0000-0002-3086-4729; Coe, Hugh/0000-0002-3264-1713 FU Norwegian Research Council FX We appreciate the useful and constructive comments and suggestions from two reviewers. This study has received support from the Norwegian Research Council. NR 67 TC 7 Z9 7 U1 0 U2 5 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0035-9009 EI 1477-870X J9 Q J ROY METEOR SOC JI Q. J. R. Meteorol. Soc. PD JAN PY 2009 VL 135 IS 638 BP 53 EP 66 DI 10.1002/qj.350 PN A PG 14 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 435WV UT WOS:000265374900004 ER PT J AU Allen, G Vaughan, G Brunner, D May, PT Heyes, W Minnis, P Ayers, JK AF Allen, G. Vaughan, G. Brunner, D. May, P. T. Heyes, W. Minnis, P. Ayers, J. K. TI Modulation of tropical convection by breaking Rossby waves SO QUARTERLY JOURNAL OF THE ROYAL METEOROLOGICAL SOCIETY LA English DT Article DE convection; tropopause fold; Rossby waves; stratosphere to troposphere exchange ID DRY-AIR; TROPOSPHERE; PACIFIC; INTRUSION; MONSOON; OZONE AB This work discusses observations of both the convective-inhibiting and convective-promoting properties associated with Rossby waves that break in the extratropics and extend into the tropics. Two tropical drought periods - times of reduced tropical cloudiness and rainfall - were observed during mid to late November 2005 over a wide area of northwest Australia, with an observed eruption of a nearby synoptic tropical cloud band in between times. Both convective inhibition and promotion appear to be linked to the descent of dry upper tropospheric air within a series of tropopause folds; convective inhibition was observed within the dry pool itself, whilst convective promotion was observed on the high moisture gradient at the leading edge of an advancing dry slot. A range of satellite images, surface rain gauges, radiosonde and ozonesonde data are used in conjunction with back trajectories and European Centre for Medium-Range Weather Forecasts (ECMWF) analysis fields to investigate the origins and dynamics associated with these convective events, showing each to be ultimately linked to breaking Rossby wave activity on the southern subtropical jet. Together, these observations support a growing number of studies linking midlatitude tropopause-level dynamics with the modulation of tropical deep convection, an influence that is poorly characterized when considering the climatology of tropical cloudiness and rainfall. Copyright (C) 2008 Royal Meteorological Society C1 [Allen, G.; Vaughan, G.; Heyes, W.] Univ Manchester, Ctr Atmospher Sci, Manchester M13 9PL, Lancs, England. [Brunner, D.] Swiss Fed Inst Mat Testing & Res, EMPA, Dubendorf, Switzerland. [May, P. T.] Ctr Australian Weather & Climate Res, Melbourne, Vic, Australia. [Minnis, P.; Ayers, J. K.] NASA, Langley Res Ctr, Sci Directorate, Hampton, VA 23665 USA. RP Allen, G (reprint author), Univ Manchester, Ctr Atmospher Sci, Oxford Rd, Manchester M13 9PL, Lancs, England. EM grant.allen@manchester.ac.uk RI Brunner, Dominik/A-1255-2009; Allen, Grant /A-7737-2013; Minnis, Patrick/G-1902-2010; Vaughan, Geraint/O-2459-2015 OI Brunner, Dominik/0000-0002-4007-6902; Allen, Grant /0000-0002-7070-3620; Minnis, Patrick/0000-0002-4733-6148; Vaughan, Geraint/0000-0002-0885-0398 NR 27 TC 15 Z9 15 U1 0 U2 9 PU JOHN WILEY & SONS LTD PI CHICHESTER PA THE ATRIUM, SOUTHERN GATE, CHICHESTER PO19 8SQ, W SUSSEX, ENGLAND SN 0035-9009 J9 Q J ROY METEOR SOC JI Q. J. R. Meteorol. Soc. PD JAN PY 2009 VL 135 IS 638 BP 125 EP 137 DI 10.1002/qj.349 PG 13 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 435WV UT WOS:000265374900010 ER PT J AU Newman, SM Knuteson, RO Zhou, DK Larar, AM Smith, WL Taylor, JP AF Newman, Stuart M. Knuteson, Robert O. Zhou, Daniel K. Larar, Allen M. Smith, William L. Taylor, Jonathan P. TI Radiative transfer validation study from the European Aqua Thermodynamic Experiment SO QUARTERLY JOURNAL OF THE ROYAL METEOROLOGICAL SOCIETY LA English DT Review DE remote sensing; AIRS; airborne measurements; spectroscopy ID SPECTROSCOPIC DATABASE; TESTBED INTERFEROMETER; RADIANCES; EAQUATE; SURFACE AB The European AQUA Thermodynamic Experiment (EAQUATE) brought together collocated hyperspectral measurements from the Atmospheric Infrared Sounder (AIRS) on NASA's Aqua satellite, as well as three airborne interferometers operating in the troposphere and stratosphere. Simultaneous observations of temperature, water vapour and trace gases have been used to constrain the atmospheric state, for validation of radiometric accuracy and radiative transfer modelling. The close agreement of observations with model spectra, in the 800-1200 cm(-1) region, indicates that the accuracy of modelling AIRS spectra is sufficient for beneficial use of the data in operational weather forecasting. The variability of atmospheric water vapour was found to be a fundamental constraint in the modelling of the 1400-1600 cm(-1) region, emphasising the requirement for a high density of observations in future validation campaigns. Copyright (C) Royal Meterological Society and Crown Copyright, 2009. C1 [Newman, Stuart M.; Taylor, Jonathan P.] Met Off, Exeter EX1 3PB, Devon, England. [Knuteson, Robert O.] Univ Wisconsin, Ctr Space Sci & Engn, Cooperat Inst Meteorol Sounding Studies, Madison, WI 53706 USA. [Zhou, Daniel K.; Larar, Allen M.] NASA, Langley Res Ctr, Hampton, VA 23665 USA. [Smith, William L.] Hampton Univ, Hampton, VA 23668 USA. RP Newman, SM (reprint author), Met Off, FitzRoy Rd, Exeter EX1 3PB, Devon, England. EM stu.newman@metoffice.gov.uk RI Zhang, YIng/F-5751-2011; Taylor, Jonathan/B-3786-2013 FU NPOESS IPO; NASA; Met Office; Natural Environment Research Council FX We thank Walter Wolf at NOAA/NESDIS and the AIRS science team for facilitating our use and analysis of AIRS data. We also thank two anonyrnous reviewers for their thorough critiques which led to improvements in the final manuscript. The NAST-I programme is supported by the NPOESS IPO, NASA Headquarters, and NASA Langley Research Center. FAAM (http://www.faam.ac.uk/) is jointly funded by the Met Office and the Natural Environment Research Council. NR 21 TC 3 Z9 3 U1 0 U2 4 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0035-9009 EI 1477-870X J9 Q J ROY METEOR SOC JI Q. J. R. Meteorol. Soc. PD JAN PY 2009 VL 135 IS 639 BP 277 EP 290 DI 10.1002/qj.382 PN B PG 14 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 435WX UT WOS:000265375100001 ER PT B AU Bartelmann, M Bennett, CL Burigana, C Chiosi, C D'Onofrio, M Dressler, A Gioia, I Hasinger, G Macias-Perez, JF Madau, P Marziani, P Mather, J Matteucci, F Olive, K Peacock, J Reich, W Robitaille, PM Rowan-Robinson, M Steigman, G Steinmetz, M Sulentic, JW Turatto, M White, SDM AF Bartelmann, Matthias Bennett, Charles L. Burigana, Carlo Chiosi, Cesare D'Onofrio, Mauro Dressler, Alan Gioia, Isabella Hasinger, Guenther Macias-Perez, Juan Francisco Madau, Piero Marziani, Paola Mather, John Matteucci, Francesca Olive, Keith Peacock, John Reich, Wolfgang Robitaille, Pierre-Marie Rowan-Robinson, Michael Steigman, Gary Steinmetz, Matthias Sulentic, Jack W. Turatto, Massimo White, Simon D. M. BE DOnofrio, M Burigana, C TI Fundamental Cosmological Observations and Data Interpretation SO QUESTIONS OF MODERN COSMOLOGY: GALILEO'S LEGACY LA English DT Article; Book Chapter ID EARLY-TYPE GALAXIES; HUBBLE-SPACE-TELESCOPE; X-RAY-CLUSTERS; MICROWAVE BACKGROUND-RADIATION; ACTIVE GALACTIC NUCLEI; COLD DARK-MATTER; PRIMORDIAL HELIUM ABUNDANCE; PROBE WMAP OBSERVATIONS; MEDIUM-SENSITIVITY SURVEY; STAR-FORMATION HISTORY C1 [Bartelmann, Matthias] Heidelberg Univ, Inst Theoret Astrophys, D-69120 Heidelberg, Germany. [Chiosi, Cesare; D'Onofrio, Mauro] Univ Padua, Dipartimento Astron, I-35122 Padua, Italy. [Burigana, Carlo] INAF Bologna, Ist Astrofis Spaziale & Fis Cosm IASF, I-40129 Bologna, Italy. [Bennett, Charles L.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Dressler, Alan] Observ Carnegie Inst Washington, Pasadena, CA 91101 USA. [Gioia, Isabella] INAF, Ist Radioastron, I-40129 Bologna, Italy. [Hasinger, Guenther] Max Planck Inst Extraterr Phys, D-85741 Garching, Germany. [Macias-Perez, Juan Francisco] Lab Phys Subatom & Cosmol, F-38026 Grenoble, France. [Madau, Piero] Univ Calif Santa Cruz, Santa Cruz, CA 95064 USA. [Marziani, Paola] Osserv Astron Padova, INAF, I-35122 Padua, Italy. [Mather, John] NASA, GSFC, Astrophys Sci Div, Greenbelt, MD 20771 USA. [Matteucci, Francesca] Univ Trieste, I-34131 Trieste, Italy. [Olive, Keith] Univ Minnesota, Sch Phys & Astron, Fine Theoret Phys Inst, Minneapolis, MN 55455 USA. [Peacock, John] Royal Observ, Inst Astron, Edinburgh EH9 3HJ, Midlothian, Scotland. [Reich, Wolfgang] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Robitaille, Pierre-Marie] Ohio State Univ, Dept Radiol, Columbus, OH 43210 USA. [Rowan-Robinson, Michael] Univ London Imperial Coll Sci Technol & Med, Blackett Lab, London SW7 2BZ, England. [Steigman, Gary] Ohio State Univ, Dept Phys, Columbus, OH 43210 USA. [Steinmetz, Matthias] Astrophys Inst Potzdam, D-14482 Potsdam, Germany. [Sulentic, Jack W.] Univ Alabama, Dept Phys & Astron, Tuscaloosa, AL 35487 USA. [Turatto, Massimo] Osserv Astrofis Catania, INAF, I-95123 Catania, Italy. [White, Simon D. M.] Max Planck Inst Astrophys, D-85740 Garching, Germany. RP Bartelmann, M (reprint author), Heidelberg Univ, Inst Theoret Astrophys, Albert Uberle Str 2, D-69120 Heidelberg, Germany. EM mbartelmann@ita.uni-heidelberg.de; cbennett@jhu.edu; burigana@iasfbo.inaf.it; cesare.chiosi@unipd.it; mauro.donofrio@unipd.it; dressler@ociw.edu; gioia@ira.inaf.it; ghasinger@mpe.mpg.de; macias@lpsc.in2p3.fr; pmadau@ucolick.org; paola.marziani@oapd.inaf.it; john.c.mather@nasa.gov; matteucci@oats.inaf.it; olive@physics.umn.edu; jap@roe.ac.uk; wreich@mpifr-bonn.mpg.de; robitaille.1@osu.edu; m.rrobinson@ic.ac.uk; steigman@mps.ohio-state.edu; msteinmetz@aip.de; jsulenti@bama.ua.edu; Massimo.Turatto@oact.inaf.it; swhite@mpa-garching.mpg.de OI Turatto, Massimo/0000-0002-9719-3157; Marziani, Paola/0000-0002-6058-4912 NR 599 TC 3 Z9 3 U1 1 U2 1 PU SPRINGER PI NEW YORK PA 233 SPRING STREET, NEW YORK, NY 10013, UNITED STATES BN 978-3-642-00791-0 PY 2009 BP 7 EP 201 DI 10.1007/978-3-642-00792-7_2 D2 10.1007/978-3-642-00792-7 PG 195 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BKX82 UT WOS:000269558100002 ER PT B AU Balbi, A Bennett, CL Bucher, M Burigana, C Coles, P D'Onofrio, M Durrer, R Mather, J Naselsky, P Perrotta, F Popa, LA Spergel, D Subramanian, K Vittorio, N AF Balbi, Amedeo Bennett, Charles L. Bucher, Martin Burigana, Carlo Coles, Peter D'Onofrio, Mauro Durrer, Ruth Mather, John Naselsky, Pavel Perrotta, Francesca Popa, Lucia A. Spergel, David Subramanian, Kandaswamy Vittorio, Nicola BE DOnofrio, M Burigana, C TI Astrophysical Cosmology SO QUESTIONS OF MODERN COSMOLOGY: GALILEO'S LEGACY LA English DT Article; Book Chapter ID MICROWAVE-ANISOTROPY-PROBE; LARGE-SCALE STRUCTURE; PRIMORDIAL MAGNETIC-FIELDS; COLD DARK-MATTER; BIG-BANG NUCLEOSYNTHESIS; DIGITAL SKY SURVEY; DOUBLE-BETA DECAY; MINIMAL ISOCURVATURE MODEL; NONZERO LEPTON NUMBERS; GALAXY REDSHIFT SURVEY C1 [Balbi, Amedeo] Univ Roma Tor Vergata, Dipartimento Fis, I-00133 Rome, Italy. [D'Onofrio, Mauro] Univ Padua, Dip Astron, I-35122 Padua, Italy. [Burigana, Carlo] INAF Bologna, Ist Astrofis Spaziale & Fis Cosm IASF, I-40129 Bologna, Italy. [Bennett, Charles L.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Bucher, Martin] Univ Paris 11, Phys Theor Lab, F-91405 Orsay, France. [Coles, Peter] Cardiff Univ, Sch Phys & Astron, Cardiff CF24 3AA, S Glam, Wales. [Naselsky, Pavel] Niels Bohr Inst, DK-2100 Copenhagen, Denmark. [Perrotta, Francesca] Osserv Astron Trieste, INAF, I-34131 Trieste, Italy. [Popa, Lucia A.] Inst Space Sci, Bucharest 76900, Romania. [Spergel, David] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. [Subramanian, Kandaswamy] Interuniv Ctr Astron & Astrophys, Pune 411007, Maharashtra, India. [Vittorio, Nicola] Univ Roma Tor Vergata, Dipartimento Fis, I-00133 Rome, Italy. [Durrer, Ruth] Univ Geneva, Dept Phys Theor, CH-1211 Geneva 4, Switzerland. [Mather, John] NASA, Astrophys Sci Div, GSFC, Greenbelt, MD 20771 USA. RP Balbi, A (reprint author), Univ Roma Tor Vergata, Dipartimento Fis, Via Ric Sci, I-00133 Rome, Italy. EM amedeo.balbi@roma2.infn.it; cbennett@jhu.edu; bucher@th.u-psud.fr; burigana@iasfbo.inaf.it; Peter.Coles@astro.cf.ac.uk; mauro.donofrio@unipd.it; Ruth.Durrer@physics.unige.ch; john.c.mather@nasa.gov; naselsky@nbi.dk; perrotta@oats.inaf.it; lpopa@venus.nipne.ro; Dns@astro.princeton.edu; kandu@iucaa.ernet.in; nicola.vittorio@roma2.infn.it RI popa, lucia/B-4718-2012 NR 276 TC 1 Z9 1 U1 0 U2 2 PU SPRINGER PI NEW YORK PA 233 SPRING STREET, NEW YORK, NY 10013, UNITED STATES BN 978-3-642-00791-0 PY 2009 BP 203 EP 299 DI 10.1007/978-3-642-00792-7_3 D2 10.1007/978-3-642-00792-7 PG 97 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BKX82 UT WOS:000269558100003 ER PT B AU Bartelmann, M Bennett, CL Bucher, M Burigana, C Capaccioli, M D'Onofrio, M Durrer, R Gioia, I Hasinger, G Lawrence, C Longo, G Macias-Perez, JF Madau, P Mather, J Peacock, J Popa, LA Rebolo, R Reich, W Steinmetz, M Turatto, M White, SDM AF Bartelmann, Matthias Bennett, Charles L. Bucher, Martin Burigana, Carlo Capaccioli, Massimo D'Onofrio, Mauro Durrer, Ruth Gioia, Isabella Hasinger, Guenther Lawrence, Charles Longo, Giuseppe Macias-Perez, Juan Francisco Madau, Piero Mather, John Peacock, John Popa, Lucia A. Rebolo, Rafael Reich, Wolfgang Steinmetz, Matthias Turatto, Massimo White, Simon D. M. BE DOnofrio, M Burigana, C TI Next Challenges SO QUESTIONS OF MODERN COSMOLOGY: GALILEO'S LEGACY LA English DT Article; Book Chapter ID DIGITAL-SKY-SURVEY; MICROWAVE BACKGROUND-RADIATION; SURVEY COMMISSIONING DATA; DARK-MATTER SUBSTRUCTURE; RAY GALAXY CLUSTERS; INFLATIONARY UNIVERSE; HIGH-REDSHIFT; COSMIC STRINGS; SCALE STRUCTURE; DATA-FLOW C1 [Bartelmann, Matthias] Univ Heidelberg, Inst Theoret Astrophys, D-69120 Heidelberg, Germany. [D'Onofrio, Mauro] Univ Padua, Dip Astron, I-35122 Padua, Italy. [Burigana, Carlo] INAF Bologna, Ist Astrofis Spaziale & Fis Cosm IASF, I-40129 Bologna, Italy. [Bennett, Charles L.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Bucher, Martin] Univ Paris 11, Phys Theor Lab, F-91405 Orsay, France. [Capaccioli, Massimo] Osserv Astron Capodimonte, VST Ctr, INAF, I-80131 Naples, Italy. [Durrer, Ruth] Univ Geneva, Dept Phys Theor, CH-1211 Geneva 4, Switzerland. [Gioia, Isabella] INAF, Ist Radioastron, I-40129 Bologna, Italy. [Hasinger, Guenther] Max Planck Inst Extraterr Phys, D-85741 Garching, Germany. [Lawrence, Charles] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Longo, Giuseppe] Univ Naples Federico 2, Dept Phys Sci, I-80126 Naples, Italy. [Macias-Perez, Juan Francisco] Lab Phys Subatom & Cosmol, F-38026 Grenoble, France. [Madau, Piero] Univ Calif Santa Cruz, Santa Cruz, CA 95064 USA. [Mather, John] NASA, Astrophys Sci Div, GSFC, Greenbelt, MD 20771 USA. [Peacock, John] Royal Observ, Inst Astron, Edinburgh EH9 3HJ, Midlothian, Scotland. [Popa, Lucia A.] Inst Space Sci, Bucharest 76900, Romania. [Rebolo, Rafael] Inst Astrofis Canarias, Tenerife 38200, Spain. [Reich, Wolfgang] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Steinmetz, Matthias] Astrophys Inst Potzdam, D-14482 Potsdam, Germany. [Turatto, Massimo] Osserv Astrofis Catania, INAF, I-95123 Catania, Italy. [White, Simon D. M.] Max Planck Inst Astrophys, D-85740 Garching, Germany. RP Bartelmann, M (reprint author), Univ Heidelberg, Inst Theoret Astrophys, Albert Uberle Str 2, D-69120 Heidelberg, Germany. EM mbartelmann@ita.uni-heidelberg.de; cbennett@jhu.edu; bucher@th.u-psud.fr; burigana@iasfbo.inaf.it; mc@na.infn.it; mauro.donofrio@unipd.it; Ruth.Durrer@physics.unige.ch; gioia@ira.inaf.it; ghasinger@mpe.mpg.de; Charles.R.Lawrence@jpl.nasa.gov; longo@na.infn.it; macias@lpsc.in2p3.fr; pmadau@ucolick.org; john.c.mather@nasa.gov; jap@roe.ac.uk; lpopa@venus.nipne.ro; rrl@iac.es; wreich@mpifr-bonn.mpg.de; msteinmetz@aip.de; Massimo.Turatto@oact.inaf.it; swhite@mpa-garching.mpg.de; burigana@iasfbo.inaf.it RI popa, lucia/B-4718-2012; OI Turatto, Massimo/0000-0002-9719-3157 NR 150 TC 0 Z9 0 U1 0 U2 2 PU SPRINGER PI NEW YORK PA 233 SPRING STREET, NEW YORK, NY 10013, UNITED STATES BN 978-3-642-00791-0 PY 2009 BP 429 EP 501 DI 10.1007/978-3-642-00792-7_5 PG 73 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BKX82 UT WOS:000269558100005 ER PT J AU Marchetti, AA McAninch, JE Rugel, G Ruhm, W Korschinek, G Martinelli, RE Faestermann, T Knie, K Egbert, SD Wallner, A Wallner, C Tanaka, K Endo, S Hoshi, M Shizuma, K Fujita, S Hasai, H Imanaka, T Straume, T AF Marchetti, A. A. McAninch, J. E. Rugel, G. Ruehm, W. Korschinek, G. Martinelli, R. E. Faestermann, T. Knie, K. Egbert, S. D. Wallner, A. Wallner, C. Tanaka, K. Endo, S. Hoshi, M. Shizuma, K. Fujita, S. Hasai, H. Imanaka, T. Straume, T. TI Fast Neutrons Measured in Copper from the Hiroshima Atomic Bomb Dome SO RADIATION RESEARCH LA English DT Article ID ACCELERATOR MASS-SPECTROMETRY; NI-63; EU-152; CO-60 AB The first measurements of (63)Ni produced by A-bomb fast neutrons (above similar to 1 MeV) in copper samples from Hiroshima encompassed distances from similar to 380 to 5062 m front the hypocenter (the point on the ground directly under the bomb). They included the region of interest to survivor studies (similar to 900 to 1500 m) and provided the first direct validation of fast neutrons in that range. However, a significant measurement gap remained between the hypocenter and 380 m. Measurements close to the hypocenter are important as a high-value anchor for the slope of the curve for neutron activation as a function of distance. Here we report measurements of (63)Ni in copper samples from the historic Hiroshima Atomic Bomb Dome, which is located similar to 150 m front the hypocenter. These measurements extend the range of our previously published data for (63)Ni providing a more comprehensive and consistent A-bomb activation curve. The results are also in good agreement with calculations based on the current dosimetry system (DS02) and give further experimental support to the accuracy of this system that forms the basis for radiation risk estimates worldwide. (C) 2009 by Radiation Research Society. C1 [Marchetti, A. A.; Martinelli, R. E.] Lawrence Livermore Natl Lab, Livermore, CA 94550 USA. [McAninch, J. E.] Los Alamos Natl Lab, Los Alamos, NM 87545 USA. [Rugel, G.; Korschinek, G.; Faestermann, T.; Knie, K.; Wallner, A.; Wallner, C.] Tech Univ Munich, Fak Phys, D-85748 Garching, Germany. [Ruehm, W.] German Res Ctr Environm Hlth, Helmholtz Zentrum Munchen, D-85764 Neuherberg, Germany. [Egbert, S. D.] Sci Applicat Int Corp, San Diego, CA 92121 USA. [Tanaka, K.; Endo, S.; Hoshi, M.; Shizuma, K.] Hiroshima Univ, Hiroshima, Japan. [Fujita, S.] Radiat Effects Res Fdn, Hiroshima, Japan. [Hasai, H.] Hiroshima Kokusai Gakuin Univ, Hiroshima, Japan. [Imanaka, T.] Kyoto Univ, Inst Res Reactor, Kyoto 6068501, Japan. [Straume, T.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Marchetti, AA (reprint author), Lawrence Livermore Natl Lab, L-096,7000 East Ave, Livermore, CA 94550 USA. EM marchetti@llnl.gov RI Wallner, Anton/G-1480-2011; Endo, Satoru/D-9091-2012; OI Wallner, Anton/0000-0003-2804-3670; Endo, Satoru/0000-0001-5961-681X; Faestermann, Thomas/0000-0002-6603-8787 FU U.S. Department of Energy [DEFG0300ER62963, DEFC0397SF21354]; U.S. National Academy of Sciences [E215099]; U.S. Army Surgeon General's Office; European Commission [FIGD-CT20000079]; German Federal Ministry of Environment; Nature Conservation and Nuclear Safety [StSch4235]; Lawrence Livermore National Laboratory [DE-AC52-07NA27344] FX We thank the Radiation Effects Research Foundation, Hiroshima University, and Hiroshima Kokusai Gakuin University for generously providing copper samples and related sample information for this study. We also thank the following organizations for supporting this work: the U.S. Department of Energy (grant DEFG0300ER62963, contract DEFC0397SF21354, TS), the U.S. National Academy of Sciences (grant E215099, TS), the U.S. Army Surgeon General's Office (TS), the European Commission (FIGD-CT20000079), the German Federal Ministry of Environment, Nature Conservation and Nuclear Safety (StSch4235). One of us (GR) would like to thank the Bavarian Government for a grant. Portions of this work were performed under the auspices of the U.S. Department of Energy by the Lawrence Livermore National Laboratory under contract DE-AC52-07NA27344. NR 17 TC 4 Z9 4 U1 1 U2 3 PU RADIATION RESEARCH SOC PI LAWRENCE PA 810 E TENTH STREET, LAWRENCE, KS 66044 USA SN 0033-7587 J9 RADIAT RES JI Radiat. Res. PD JAN PY 2009 VL 171 IS 1 BP 118 EP 122 DI 10.1667/RR1436.1 PG 5 WC Biology; Biophysics; Radiology, Nuclear Medicine & Medical Imaging SC Life Sciences & Biomedicine - Other Topics; Biophysics; Radiology, Nuclear Medicine & Medical Imaging GA 390TX UT WOS:000262187700012 PM 19138052 ER PT S AU Liechty, DS AF Liechty, Derek S. BE Abe, T TI Modifications to Axially Symmetric Simulations Using New DSMC (2007) Algorithms SO RAREFIED GAS DYNAMICS SE AIP Conference Proceedings LA English DT Proceedings Paper CT 26th International Symposium on Rarefied Gas Dynamics (RGD26) CY JUN 20-JUL 25, 2008 CL Kyoto, JAPAN SP Japan Soc Promot Sci, Japan Aerosp Explorat Agcy, Soc Promot Space Sci, Iwantani Naoji Fdn, Inoue Fdn Sci, Casio Sci Promot Fdn, Kaijma Fdn, IHI Corp, IHI Aerosp Engn Co Ltd, Osaka Vaccuun Ltd, Nissin Inc DE Monte Carlo; particle methods; nonequilibrium fluid. AB Several modifications aimed at improving physical accuracy are proposed for solving axially symmetric problems building on the DSMC (2007) algorithms introduced by Bird. Originally developed to solve nonequilibrium, rarefied flows, the DSMC method is now regularly used to solve complex problems over a wide range of Knudsen numbers. These new algorithms include features such as nearest neighbor collisions excluding the previous collision partners, separate collision and sampling cells, automatically adaptive variable time steps, a modified no-time counter procedure for collisions, and discontinuous and event-driven physical processes. Axially symmetric solutions require radial weighting for the simulated molecules since the molecules near the axis represent fewer real molecules than those farther away from the axis due to the difference in volume of the cells. In the present methodology, these radial weighting factors are continuous, linear functions that vary with the radial position of each simulated molecule. It is shown that how one defines the number of tentative collisions greatly influences the mean collision time near the axis. The method by which the grid is treated for axially symmetric problems also plays an important role near the axis, especially for scalar pressure. A new method to treat how the molecules are traced through the grid is proposed to alleviate the decrease in scalar pressure at the axis near the surface. Also, a modification to the duplication baffler is proposed to vary the duplicated molecular velocities while retaining the molecular kinetic energy and axially symmetric nature of the problem. C1 NASA, Langley Res Ctr, Aerothermodynam Branch, Hampton, VA 23681 USA. RP Liechty, DS (reprint author), NASA, Langley Res Ctr, Aerothermodynam Branch, Hampton, VA 23681 USA. NR 7 TC 0 Z9 0 U1 0 U2 0 PU AMER INST PHYSICS PI MELVILLE PA 2 HUNTINGTON QUADRANGLE, STE 1NO1, MELVILLE, NY 11747-4501 USA SN 0094-243X BN 978-0-7354-0615-5 J9 AIP CONF PROC PY 2009 VL 1084 BP 251 EP 256 PG 6 WC Engineering, Aerospace; Physics, Fluids & Plasmas SC Engineering; Physics GA BJF97 UT WOS:000265564800040 ER PT S AU Goldstein, DB Summy, D Colaprete, A Varghese, PL Trafton, LM AF Goldstein, D. B. Summy, D. Colaprete, A. Varghese, P. L. Trafton, L. M. BE Abe, T TI Modeling the Vapor and Dust Dynamics Due to the Impact of the LCROSS Spacecraft on the Moon. SO RAREFIED GAS DYNAMICS SE AIP Conference Proceedings LA English DT Proceedings Paper CT 26th International Symposium on Rarefied Gas Dynamics (RGD26) CY JUN 20-JUL 25, 2008 CL Kyoto, JAPAN SP Japan Soc Promot Sci, Japan Aerosp Explorat Agcy, Soc Promot Space Sci, Iwantani Naoji Fdn, Inoue Fdn Sci, Casio Sci Promot Fdn, Kaijma Fdn, IHI Corp, IHI Aerosp Engn Co Ltd, Osaka Vaccuun Ltd, Nissin Inc DE Collisionless atmosphere; exosphere; lunar atmosphere; lunar impact ID LUNAR SOUTH-POLE; WATER ICE; COLD TRAP; DEPOSITS; PROSPECTOR; SEARCH AB The implications of possibly large volatile reservoirs on the Moon are significant for the future of manned activity there and for space science and exploration in general. In autumn of 2008 NASA will launch the LCROSS mission to impact two spacecraft into a permanently shadowed crater-a cold trap - at the south pole of the Moon. The lead spacecraft will excavate its own several meter crater. The process will be observed by the following smaller vehicle and by orbiting and Earth-based instruments in hopes of observing the release of volatiles-predominantly water -- from the lunar soil. The following vehicle will then impact as well. We examine the plausible vapor dynamics following the impacts and concentrate on the observability of the gas from Earth or lunar orbit. In the free-molecular computational model of the vapor motion, water and OH molecules move ballistically, have a temperature-dependent surface residence time, and are subject to photo-dissociation and ionization losses. Sunlight shadowing, separation of the vapor from the dust grains, dust thermodynamics and different impact plume models are considered. C1 [Goldstein, D. B.; Summy, D.; Varghese, P. L.; Trafton, L. M.] Univ Texas Austin, Austin, TX 78712 USA. [Colaprete, A.] NASA, Ames Res Ctr, Moffett Field, CA USA. RP Goldstein, DB (reprint author), Univ Texas Austin, Austin, TX 78712 USA. FU NASA [NNG04GQ66G, NNX08AZ42A] FX This work was supported in part by NASA grants NNG04GQ66G and NNX08AZ42A. NR 24 TC 2 Z9 2 U1 0 U2 1 PU AMER INST PHYSICS PI MELVILLE PA 2 HUNTINGTON QUADRANGLE, STE 1NO1, MELVILLE, NY 11747-4501 USA SN 0094-243X BN 978-0-7354-0615-5 J9 AIP CONF PROC PY 2009 VL 1084 BP 1061 EP + PG 2 WC Engineering, Aerospace; Physics, Fluids & Plasmas SC Engineering; Physics GA BJF97 UT WOS:000265564800170 ER PT B AU Scimemi, SJ AF Scimemi, Samuel J. BE Kurnaz, S Ince, F Onbasioglu, S Basturk, S TI Human Space Flight Docking Interoperability SO RAST 2009: PROCEEDINGS OF THE 4TH INTERNATIONAL CONFERENCE ON RECENT ADVANCES IN SPACE TECHNOLOGIES LA English DT Proceedings Paper CT 4th International Conference on Recent Advances in Space Technologies CY JUN 11-13, 2009 CL Istanbul, TURKEY SP turkish Air Force Acad, Istanbul Tech Univ, Bogazici Univ, Marmara Univ, Bahcesehir Univ, Istanbul Commerce Univ, Halic Univ, Yeditepe Univ, IEEE, AIAA C1 NASA Headquarters, Washington, DC 20009 USA. RP Scimemi, SJ (reprint author), NASA Headquarters, 300 E St SW,Suite 7A16, Washington, DC 20009 USA. EM sam.scimemi@nasa.gov NR 0 TC 0 Z9 0 U1 0 U2 0 PU IEEE PI NEW YORK PA 345 E 47TH ST, NEW YORK, NY 10017 USA BN 978-1-4244-3626-2 PY 2009 BP 167 EP 169 DI 10.1109/RAST.2009.5158189 PG 3 WC Engineering, Aerospace SC Engineering GA BLZ72 UT WOS:000271613000034 ER PT S AU Dorodnitsyn, A Kallman, T AF Dorodnitsyn, A. Kallman, T. BE Hubeny, I Stone, JM MacGregor, K Werner, K TI The formation of narrow X-ray line spectra from realistic hydrodynamical models: applications to the problem of warm absorbers SO RECENT DIRECTIONS IN ASTROPHYSICAL QUANTITATIVE SPECTROSCOPY AND RADIATION HYDRODYNAMICS SE AIP Conference Proceedings LA English DT Proceedings Paper CT Conference on Recent Directions in Astrophysical Quantitative Spectroscopy and Radiation Hydrodynamics held in honor of Dimitri Mihalas CY MAR 30-APR 03, 2009 CL Boulder, CO SP Natl Ctr Atmospher Res DE Document processing; Class file writing; LATEX2 epsilon AB We calculate a series of synthetic spectra from outflows originating from the obscuring torus in active galactic nuclei (AGN). Such modeling includes 2.5D hydrodynamical simulations of an X-ray excited torus wind, including the effects of X-ray heating, ionization, and radiation pressure. 3D radiation transfer calculations are performed in the 3D Sobolev approximation. Synthetic X-ray line spectra and individual profiles of several strong lines are shown at different inclination angles, observing times, and for different characteristics of the torus. C1 [Dorodnitsyn, A.; Kallman, T.] NASA, Goddard Space Flight Ctr, High Energy Astrophys Lab, Greenbelt, MD 20771 USA. RP Dorodnitsyn, A (reprint author), NASA, Goddard Space Flight Ctr, High Energy Astrophys Lab, Code 662, Greenbelt, MD 20771 USA. NR 2 TC 0 Z9 0 U1 0 U2 0 PU AMER INST PHYSICS PI MELVILLE PA 2 HUNTINGTON QUADRANGLE, STE 1NO1, MELVILLE, NY 11747-4501 USA SN 0094-243X BN 978-0-7354-0710-7 J9 AIP CONF PROC PY 2009 VL 1171 BP 304 EP 308 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BQB69 UT WOS:000280587500027 ER PT S AU Garcia, J Kallman, T AF Garcia, Javier Kallman, Tim BE Hubeny, I Stone, JM MacGregor, K Werner, K TI Comptonized Fe K-lines in the X-ray spectra of Low-Mass X-ray Binaries SO RECENT DIRECTIONS IN ASTROPHYSICAL QUANTITATIVE SPECTROSCOPY AND RADIATION HYDRODYNAMICS SE AIP Conference Proceedings LA English DT Proceedings Paper CT Conference on Recent Directions in Astrophysical Quantitative Spectroscopy and Radiation Hydrodynamics held in honor of Dimitri Mihalas CY MAR 30-APR 03, 2009 CL Boulder, CO SP Natl Ctr Atmospher Res DE accretion, accretion disks; line: formation; radiative transfer; X-rays: binaries ID IRON; PHOTOIONIZATION; REFLECTION AB We present new models for the vertical structure of accretion disks illuminated by X-rays. The chief advance is the inclusion of the most recent atomic data for the inner-shell of the iron isonuclear sequence. We also include the redistribution of the photons due to Compton scattering. By performing detailed ID radiative transfer calculations, we have computed the reflected spectra from constant density slabs for different degrees of ionization. Our results show that Comptonization can be responsible for a significant fraction of the broadening of the Fe K-line. This is of interest in view of recent observations which have revealed broad and asymmetric iron emission line profiles in some neutron star Low Mass X-Ray Binaries (LMXBs). Although these resemble the broadened lines observed in some active galactic nuclei, and which are likely due to the Doppler effect and gravitational redshift, we examine the contribution to the Fe K-line broadening by Comptonization in a disk atmosphere. Using simulated Suzaku observations, we compare our models with the current C1 [Garcia, Javier] Catholic Univ Amer, IACS, Dept Phys, Washington, DC 20064 USA. [Kallman, Tim] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Garcia, J (reprint author), Catholic Univ Amer, IACS, Dept Phys, Washington, DC 20064 USA. NR 7 TC 0 Z9 0 U1 0 U2 0 PU AMER INST PHYSICS PI MELVILLE PA 2 HUNTINGTON QUADRANGLE, STE 1NO1, MELVILLE, NY 11747-4501 USA SN 0094-243X BN 978-0-7354-0710-7 J9 AIP CONF PROC PY 2009 VL 1171 BP 363 EP + PG 2 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BQB69 UT WOS:000280587500042 ER PT S AU Shen, SH Leptoukh, G Loboda, T Csiszar, I Romanov, P Gerasimov, I AF Shen, Suhung Leptoukh, Gregory Loboda, Tatiana Csiszar, Ivan Romanov, Peter Gerasimov, Irina BE Groisman, PY Ivanov, SV TI The NASA NEESPI Data Portal to Support Studies of Climate and Environmental Changes in Non-boreal Europe SO REGIONAL ASPECTS OF CLIMATE-TERRESTRIAL-HYDROLOGIC INTERACTIONS IN NON-BOREAL EASTERN EUROPE SE NATO Science for Peace and Security Series C-Environmental Security LA English DT Proceedings Paper CT NATO Advanced Research Workshop on Regional Aspects of Climate-Terrestrial-Hydrologic Interactions in Non-boreal Eastern Europe CY AUG 23-28, 2008 CL Odessa, UKRAINE SP NATO, No Eurasia Earth Sci Partnership Initiat DE remote sensing; online visualization; data analysis; fire; NDVI AB Goddard Interactive Online Visualization ANd aNalysis Infrastructure (Giovanni) data portal is ready to support NEESPI studies in Northern Eurasia with high quality remote sensing information. C1 [Shen, Suhung] George Mason Univ, Data & Informat Serv Ctr, NASA, GSFC, Code 610-2, Greenbelt, MD 20771 USA. [Leptoukh, Gregory] NASA, GSFC, Greenbelt, MD 20771 USA. [Loboda, Tatiana; Csiszar, Ivan; Romanov, Peter] Univ Maryland, College Pk, MD 20742 USA. [Gerasimov, Irina] NASA, GSFC, ADNET, Greenbelt, MD 20771 USA. RP Shen, SH (reprint author), George Mason Univ, Data & Informat Serv Ctr, NASA, GSFC, Code 610-2, Greenbelt, MD 20771 USA. EM suhung.shen-1@nasa.gov RI Csiszar, Ivan/D-2396-2010; Romanov, Peter/F-5622-2010 OI Romanov, Peter/0000-0002-2153-8307 FU NASA through ROSES [NNH05ZDA001N-ACCESS] FX The project is supported by NASA through ROSES 2005 NNH05ZDA001N-ACCESS. The authors wish to express great appreciation for the technical support of the Giovanni software development and S4PA data ingest working groups at NASA GES-DISC. NR 9 TC 1 Z9 1 U1 0 U2 2 PU SPRINGER PI DORDRECHT PA PO BOX 17, 3300 AA DORDRECHT, NETHERLANDS SN 1871-4668 BN 978-481-2241-7; 978-90-481-2240-0 J9 NATO SCI PEACE SECUR JI NATO Sci. Peace Secur. Ser. C- Environ. Secur. PY 2009 BP 9 EP + DI 10.1007/978-90-481-2283-7_2 PG 2 WC Environmental Sciences; Meteorology & Atmospheric Sciences SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences GA BJK38 UT WOS:000266662700002 ER PT S AU Gutman, G AF Gutman, Garik BE Groisman, PY Ivanov, SV TI The NASA Land-Cover/Land-Use Change (LCLUC) Program's Support of the Northern Eurasia Earth Science Partnership Initiative (NEESPI): Focus on Non-boreal Europe SO REGIONAL ASPECTS OF CLIMATE-TERRESTRIAL-HYDROLOGIC INTERACTIONS IN NON-BOREAL EASTERN EUROPE SE NATO Science for Peace and Security Series C - Environmental Security LA English DT Proceedings Paper CT NATO Advanced Research Workshop on Regional Aspects of Climate-Terrestrial-Hydrologic Interactions in Non-boreal Eastern Europe CY AUG 23-28, 2008 CL Odessa, UKRAINE SP NATO, No Eurasia Earth Sci Partnership Initiat DE land cover; land use change; non-boreal Eastern Europe ID BIOOPTICAL PARAMETER VARIABILITY; CHLOROPHYLL-A CONCENTRATION; TURBID PRODUCTIVE WATERS; GYPSY-MOTH DEFOLIATION; REMOTE ESTIMATION; FOREST DISTURBANCE AB Currently, the Northern Eurasia Earth Science Partnership Initiative (NEESPI) includes over 120 international projects involving more than 200 scientific institutions from over 30 countries. The program involves national government agencies, academia and private organizations in the U.S., Europe, Japan and Northern Eurasia (Gutman 2007). The NEESPI science is directed at evaluating the role of anthropogenic impacts on the Northern Eurasia ecosystems, the hemispheric-scale interaction and assessing how future human actions would affect the global climate and ecosystems of the region. Projections of the consequences of global changes for regional environment in Northern Eurasia are also in the center of the scientific foci of this initiative. The Land-Cover/Land-Use Change (LCLUC) Program is an interdisciplinary science program in the Earth Science Division of the Science Mission Directorate supporting several regional initiatives, including NEESPI. The NASA LCLUC currently funds over 30 NEESPI projects. The NEESPI program links to several international projects, such as GLP, iLEAPS and others, under major international programs: IGBP and WCRP. The NEESPI covers a large geographic domain, which includes the former Soviet Union, northern China, Mongolia, Scandinavia and Eastern Europe. This contribution provides a short description of the ongoing NEESPI studies in the non-boreal European sub-region of the NEESPI geographic domain that are supported by the NASA LCLUC program. More information on the projects can be found at http://neespi.org and http://lcluc.hq.nasa.gov. C1 NASA Headquarters, Land Cover Land Use Change Program, Washington, DC 20546 USA. RP Gutman, G (reprint author), NASA Headquarters, Land Cover Land Use Change Program, 300 E St SW, Washington, DC 20546 USA. EM ggutman@noaa.gov NR 18 TC 0 Z9 0 U1 0 U2 0 PU SPRINGER PI DORDRECHT PA PO BOX 17, 3300 AA DORDRECHT, NETHERLANDS SN 1871-4668 BN 978-481-2241-7 J9 NATO SCI PEACE SECUR PY 2009 BP 117 EP 122 DI 10.1007/978-90-481-2283-7_13 PG 6 WC Environmental Sciences; Meteorology & Atmospheric Sciences SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences GA BJK38 UT WOS:000266662700013 ER PT S AU Ramesham, R AF Ramesham, Rajeshuni BE Kullberg, RC Ramesham, R TI Environmental Testing of COTS Components for Space Applications SO RELIABILITY, PACKAGING, TESTING, AND CHARACTERIZATION OF MEMS/MOEMS AND NANODEVICES VIII SE Proceedings of SPIE-The International Society for Optical Engineering LA English DT Proceedings Paper CT Conference on Reliability, Packaging, Testing, and Characterization of MEMS/MOEMS and Nanodevices VIII CY JAN 28-29, 2009 CL San Jose, CA SP SPIE, Texas Instruments Inc, Nanoink Inc, Photon Ctr Boston Univ, Ozen Engn Inc DE COTS; MEMS; Life testing; Protoflight qualification; Valves; Pumps; and Reliability ID RELIABILITY; MEMS AB Research and development of microelectromechanical systems (MEMS) has shown a significant promise for a variety of commercial applications. For example, accelerometers are widely used for air bags in automobiles, MEMS inkjet print heads are used for printers, gyroscopes for guidance and navigation and pressure sensors for various industrial applications. Some of the MEMS devices have potential to become the commercial-off-the-shelf (COTS) components. Aerospace requires more sophisticated technology development to achieve significant cost savings if they could utilize COTS components in their systems. A miniature gas chromatograph instrument designed as a space station project will provide on-orbit detection, identification, and quantification of potentially toxic trace volatile organic compounds in the human-supporting environment. The instrument consists of several commercial off-the-shelf (COTS) valves, pumps and sensors. This paper describes the thermal environmental requirements and protoflight/qualification thermal test results for the COTS parts at cold and hot temperature extremes. The objective of this study is to qualify several COTS components for specific thermal/dynamic environments to assess their reliability. All COTS components life tested were believed to meet the 3x mission operational life requirements. Test results will be presented. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Ramesham, R (reprint author), CALTECH, Jet Prop Lab, 125-204D,4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM Rajeshuni.ramesham@jpl.nasa.gov; Rajeshuni.ramesham@jpl.nasa.gov NR 30 TC 0 Z9 0 U1 1 U2 4 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 978-0-8194-7452-0 J9 P SOC PHOTO-OPT INS PY 2009 VL 7206 AR 72060H DI 10.1117/12.813408 PG 11 WC Nanoscience & Nanotechnology; Materials Science, Characterization & Testing; Optics SC Science & Technology - Other Topics; Materials Science; Optics GA BSP99 UT WOS:000285331000016 ER PT S AU Lin, B Fan, TF AF Lin, Bing Fan, Tai-Fang (Alice) BE Revetria, R Mladenov, V Mastorakis, N TI Global Atmospheric Heat Distributions Observed From Space SO REMOTE'09: PROCEEDINGS OF THE 5TH WSEAS INTERNATIONAL CONFERENCE ON REMOTE SENSING SE Mathematics and Computers in Science and Engineering LA English DT Proceedings Paper CT 5th WSEAS International Conference on Remote Sensing (REMOTE '09) CY OCT 17-19, 2009 CL Univ Genova, Genoa, ITALY SP WSEAS HO Univ Genova DE radiation; latent heat; sensible heat; satellite observation AB This study focuses on the observations of global atmospheric heat distributions using satellite measurements. Major heat components such as radiation energy, latent heat and sensible heat are considered. The uncertainties and error sources are assessed. Results show that the atmospheric heat is basically balanced, and the observed patterns of radiation and latent heat from precipitation are clearly related to general circulation. C1 [Lin, Bing] NASA, Sci Directorate, Langley Res Ctr, Hampton, VA 23681 USA. [Fan, Tai-Fang (Alice)] SSSAI, Hampton, VA 23666 USA. RP Lin, B (reprint author), NASA, Sci Directorate, Langley Res Ctr, Hampton, VA 23681 USA. EM Bing.Lin@nasa.gov; Tai-Fang.Fan-1@nasa.gov NR 2 TC 0 Z9 0 U1 0 U2 0 PU WORLD SCIENTIFIC AND ENGINEERING ACAD AND SOC PI ATHENS PA AG LOANNOU THEOLOGOU 17-23, 15773 ZOGRAPHOU, ATHENS, GREECE SN 1792-4308 BN 978-960-474-129-8 J9 MATH COMPUT SCI ENG PY 2009 BP 19 EP 21 PG 3 WC Remote Sensing SC Remote Sensing GA BOF41 UT WOS:000276454400002 ER PT B AU Hu, YX AF Hu, Yongxiang BE Revetria, R Mladenov, V Mastorakis, N TI Ocean, Land and Meteorology Studies Using Space-Based Lidar Measurements SO REMOTE'09: PROCEEDINGS OF THE 5TH WSEAS INTERNATIONAL CONFERENCE ON REMOTE SENSING SE Mathematics and Computers in Science and Engineering LA English DT Proceedings Paper CT 5th WSEAS International Conference on Remote Sensing (REMOTE '09) CY OCT 17-19, 2009 CL Univ Genova, Genoa, ITALY SP WSEAS HO Univ Genova DE lidar ocean wind aerosol temperature altimetry ID SURFACE AB CALIPSO's main mission objective is studying the climate impact of clouds and aerosols in the atmosphere. CALIPSO also collects information about other components of the Earth's ecosystem, such as oceans and land. This paper introduces the physics concepts and presents preliminary results for the valueadded CALIPSO Earth system science products. These include ocean surface wind speeds, column atmospheric optical depths, ocean subsurface backscatter, land surface elevations, atmospheric temperature profiles, and A-train data fusion products. C1 NASA, Langley Res Ctr, Hampton, VA 23681 USA. RP Hu, YX (reprint author), NASA, Langley Res Ctr, MS 475, Hampton, VA 23681 USA. EM Yongxiang.hu-1@nasa.gov RI Hu, Yongxiang/K-4426-2012 NR 6 TC 0 Z9 0 U1 0 U2 0 PU WORLD SCIENTIFIC AND ENGINEERING ACAD AND SOC PI ATHENS PA AG LOANNOU THEOLOGOU 17-23, 15773 ZOGRAPHOU, ATHENS, GREECE BN 978-960-474-129-8 J9 MATH COMPUT SCI ENG PY 2009 BP 47 EP 50 PG 4 WC Remote Sensing SC Remote Sensing GA BOF41 UT WOS:000276454400007 ER PT B AU Xu, KM Su, WY Eitzen, Z AF Xu, Kuan-Man Su, Wenying Eitzen, Zachary BE Revetria, R Mladenov, V Mastorakis, N TI Use of CERES Cloud and Radiation Data for Model Evaluation and Cloud Feedback Studies SO REMOTE'09: PROCEEDINGS OF THE 5TH WSEAS INTERNATIONAL CONFERENCE ON REMOTE SENSING SE Mathematics and Computers in Science and Engineering LA English DT Proceedings Paper CT 5th WSEAS International Conference on Remote Sensing (REMOTE '09) CY OCT 17-19, 2009 CL Univ Genova, Genoa, ITALY SP WSEAS HO Univ Genova DE CERES; Cloud Feedback; Cloud Radiative Effects ID SURFACE-TEMPERATURE AB The availability of enormous amounts of satellite remote sensing data provides a golden opportunity to improve the capability of climate models for projecting future climate change. In this study, we will present recent progress in using CERES (Clouds and the Earth's Radiant Energy System) satellite data to evaluate model performance with regards to the vertical structures of radiative fluxes and cloud radiative effects and to provide an unambiguous estimate of the magnitude of low cloud feedbacks. C1 [Xu, Kuan-Man; Su, Wenying; Eitzen, Zachary] NASA, Langley Res Ctr, Climate Sci Branch, Hampton, VA 23681 USA. RP Xu, KM (reprint author), NASA, Langley Res Ctr, Climate Sci Branch, Mail Stop 420, Hampton, VA 23681 USA. EM Kuan-Man.Xu@nasa.gov; Wenying.Su-1@nasa.gov; Zachary.A.Eitzen@nasa.gov RI Xu, Kuan-Man/B-7557-2013 OI Xu, Kuan-Man/0000-0001-7851-2629 NR 16 TC 0 Z9 0 U1 0 U2 3 PU WORLD SCIENTIFIC AND ENGINEERING ACAD AND SOC PI ATHENS PA AG LOANNOU THEOLOGOU 17-23, 15773 ZOGRAPHOU, ATHENS, GREECE BN 978-960-474-129-8 J9 MATH COMPUT SCI ENG PY 2009 BP 56 EP 61 PG 6 WC Remote Sensing SC Remote Sensing GA BOF41 UT WOS:000276454400009 ER PT S AU Taranik, JV Coolbaugh, MF Vaughan, RG AF Taranik, James V. Coolbaugh, Mark F. Vaughan, R. Greg BE Bedell, R Crosta, AP Grunsky, E TI An Overview of Thermal Infrared Remote Sensing with Applications to Geothermal and Mineral Exploration in the Great Basin, Western United States SO REMOTE SENSING AND SPECTRAL GEOLOGY SE Reviews in Economic Geology LA English DT Article; Book Chapter ID REFLECTION RADIOMETER ASTER; MULTISPECTRAL SCANNER; VIRGINIA RANGE; DEATH-VALLEY; LAVA FLOWS; IMAGES; NEVADA; CALIFORNIA; EMISSION; AIRBORNE AB The physics of thermal infrared aerospace measurements is based on Planck's Radiation law,, Wien's Displacement law, and Kirchoff's law. The electromagnetic spectrum for thermal infrared aerospace measurements includes measurements beyond the reflected short- (2.5 mu m) to the long-wave infrared (14 mu m). Thermal infrared sensors measure thermal emission from the Earths surface in single wavelength bands (broadband), tens of bands (multiband), and in hundreds of hands (hyperspectral). Broadband thermal infrared measurement techniques include surface temperature Mapping and thermal inertia mapping. Multiband and hyperspectral techniques involve mapping of changes in thermal emission at different wavelengths (emissivity mapping). Today, broadband surface temperature mapping is mostly done with satellite sensors. Thermal inertia mapping is done using broadband measurements taken during the day and night. Emissivity mapping is done using tens to hundreds of hands, and it requires sensors capable of measuring small changes in radiant emittance. Sensor systems discussed in this study include: Thermal Infrared Multispectral Scanner (TIMS), the Moderate Resolution Imaging Spectroradiometer (MODIS), Advanced Spaceborne Thermal Emission and Reflection Radiometer (ASTER) Simulator (MASTER), the Spatially Enhanced Broadband Array Spectrograph System (SEBASS) and the ASTER satellite sensor. Several areas of Nevada, such as Brady's Hot Springs, Steamboat Springs, Geiger Grade, and Virginia City, were used as sites for demonstrating the geologic applications of thermal infrared remote sensing. Corrected day and night images over Steamboat Springs were acquired by TIMS. These day-night images were combined together to produce a final processed temperature image, in which the temperature effects of albedo, topographic slope, and thermal inertia were minimized to facilitate the detection of geothermal anomalies. Spectral variations in emitted thermal energy were detected over the Geiger Grade and Virginia City areas Using the MODIS-ASTER Simulator (MASTER) and (SEBASS). MASTER thermal infrared image data allowed two primary mineralogic units in the Steamboat. Springs area to he identified: sinter and/or chalcedony deposits and quartz-alunite allteration, which have spectral emissivity features around 9.0 mu m; and clay-rich soil and clay alteration, which have spectral emissivity features around 9.7 mu m. The higher spatial and spectral resolution SEBASS data allowed six different alteration assemblages to be identified: quartz, alunite, pyrophyllite, feldspar, kaolinite, and montmorillonite and/or illite. C1 [Taranik, James V.] Univ Nevada, Arthur Brant Lab Explorat Geophys, Mackay Sch Earth Sci & Engn, Reno, NV 89557 USA. [Vaughan, R. Greg] Planetary Sci Inst, Tucson, AZ 85719 USA. [Taranik, James V.] NASA Headquarters, Off Space & Terr Applicat, Washington, DC USA. [Vaughan, R. Greg] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Taranik, James V.] NASA, Washington, DC USA. [Coolbaugh, Mark F.] Univ Nevada, Great Basin Ctr Geothermal Energy, Reno, NV 89557 USA. RP Taranik, JV (reprint author), Univ Nevada, Arthur Brant Lab Explorat Geophys, Mackay Sch Earth Sci & Engn, Reno, NV 89557 USA. EM jtaraink@mines.unr.edu NR 80 TC 3 Z9 3 U1 1 U2 5 PU SOC ECONOMIC GEOLOGISTS, INC PI LITTLETON PA 7811 SHAFFER PKWY, LITTLETON, CO 80127 USA SN 0741-0123 BN 978-1-934969-13-7 J9 REV ECON GEOL PY 2009 VL 16 BP 41 EP 57 PG 17 WC Geology; Remote Sensing; Mining & Mineral Processing SC Geology; Remote Sensing; Mining & Mineral Processing GA BKK76 UT WOS:000268394400006 ER PT S AU Taranik, JV Aslett, ZL AF Taranik, James V. Aslett, Zan L. BE Bedell, R Crosta, AP Grunsky, E TI Development of Hyperspectral Imaging for Mineral Exploration SO REMOTE SENSING AND SPECTRAL GEOLOGY SE Reviews in Economic Geology LA English DT Article; Book Chapter ID SPECTROMETER AVIRIS; EO-1 HYPERION; AIRBORNE; SPECTROSCOPY; EARTH; SPECTRORADIOMETER; NEVADA; IMAGES AB The emergence of hyperspectral image data to remotely map minerals oil the surface of the Earth is the result of decades of laboratory, engineering, and physics research conducted by both commercial and government sectors. We present a synopsis of major events which culminated ill the development of mature hyperspectral reflectance and thermal emissivity data collection capabilities that are Currently available in worldwide capacity. Laboratory and field measurement efforts in the 1960s produced a foundation of knowledge pertaining to mineral spectral phenomenology. This in turn spurred the creation of first broadband multispectral and then hyperspectral data via airborne and spaceborne sensors to capitalize on mineral characteristics. Highly accurate radiometric calibration and atmospheric corrections allow remote measurements to closely emulate ground or laboratory measurements, while commercial hyperspectral data processing software enables timely analysis of the data. Increasing amounts of image data have been collected by a variety of commercial and government sensors, of which mineral exploration is a predominant application. The differences in sensor mid image data acquisition parameters directly affect the ability to map minerals. A brief analysis of Cuprite, Nevada, using multiple sensors is used as all example to illuminate factors of importance. C1 [Taranik, James V.; Aslett, Zan L.] Univ Nevada, Arthur Brant Lab Explorat Geophys ABLE, Mackay Sch Earth Sci & Engn, Reno, NV 89557 USA. [Taranik, James V.] NASA Headquarters, Off Space & Terr Applicat, Washington, DC USA. [Taranik, James V.] NASA, Washington, DC USA. RP Taranik, JV (reprint author), Univ Nevada, Arthur Brant Lab Explorat Geophys ABLE, Mackay Sch Earth Sci & Engn, Mail Stop 168, Reno, NV 89557 USA. EM jtaranik@mines.unr.edu NR 43 TC 7 Z9 7 U1 0 U2 2 PU SOC ECONOMIC GEOLOGISTS, INC PI LITTLETON PA 7811 SHAFFER PKWY, LITTLETON, CO 80127 USA SN 0741-0123 BN 978-1-934969-13-7 J9 REV ECON GEOL PY 2009 VL 16 BP 83 EP 95 PG 13 WC Geology; Remote Sensing; Mining & Mineral Processing SC Geology; Remote Sensing; Mining & Mineral Processing GA BKK76 UT WOS:000268394400008 ER PT S AU Gentile, A Pierce, L Ciraolo, G Zhang, G La Loggia, G Nemani, R AF Gentile, A. Pierce, L. Ciraolo, G. Zhang, G. La Loggia, G. Nemani, R. BE Neale, CMU Maltese, A TI Comparison between energy balance and mass balance models for actual evapotranspiration assessment SO REMOTE SENSING FOR AGRICULTURE, ECOSYSTEMS, AND HYDROLOGY XI SE Proceedings of SPIE LA English DT Proceedings Paper CT Conference on Remote Sensing for Agriculture, Ecosystems and Hydrology XI as Part of the 16th International Symposium on Remote Sensing CY AUG 31-SEP 03, 2009 CL Berlin, GERMANY SP SPIE Europe DE evapotranspiration; surface energy balance; water balance; viticulture; Landsat 5 ID MAPPING EVAPOTRANSPIRATION; VINEYARD; SOIL AB The assessment of the water needs for a specific crop has a fundamental importance in the management of water resources. The application of empirical models able to retrieve estimates of the actual evapotranspiration (ETa) to assess the need for water could give a valid tool for the planning of water supply, avoiding unnecessary water losses. In this context, two independent models for estimating actual evapotranspiration were compared. The first model is based on an energy balance and uses remotely sensed data and ancillary data from weather stations to assess the ETa. The second model also uses remotely sensed data and climatic data on a daily basis from a weather network. Field measurements are needed to calibrate both models. The study was conducted in a commercial vineyard located in Napa Valley (California). The observed range of ETdaily is included within the values measured by other authors. The results retrieved from both models show actual ETdaily values with a different trend over time; after mid-summer (early July) VSIM estimates of ETdaily trend downwards, while SEBAL estimates remain fairly constant. This disagreement illustrate the difficulty in estimating the actual evapotranspiration at the end of season, when soil moisture gets low and vine water stress increases due to reducing stomatal conductance. C1 [Gentile, A.; Ciraolo, G.; La Loggia, G.] Univ Palermo, DIIAA, Dept Hydraul Engn & Environm Applicat, I-90133 Palermo, Italy. [Pierce, L.] Calif State Univ Monterey Bay, Div Sci & Environm Policy, Monterey, CA 93933 USA. [Zhang, G.] Utah State Univ, Dept Watershed Sci, Logan, UT 84322 USA. [Nemani, R.] NASA, Ames Res Ctr, Div Earth Sci, Moffett Field, CA 94035 USA. RP Gentile, A (reprint author), Univ Palermo, DIIAA, Dept Hydraul Engn & Environm Applicat, I-90133 Palermo, Italy. OI Ciraolo, Giuseppe/0000-0001-6627-0175 NR 22 TC 0 Z9 0 U1 1 U2 4 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 978-0-8194-7777-4 J9 PROC SPIE PY 2009 VL 7472 AR 747212 DI 10.1117/12.830229 PG 12 WC Agricultural Engineering; Remote Sensing; Optics SC Agriculture; Remote Sensing; Optics GA BDH76 UT WOS:000313294600025 ER PT S AU Kassianov, E Ovchinnikov, M Berg, LK McFarlane, SA Flynn, C Ferrare, R Hostetler, C AF Kassianov, Evgueni Ovchinnikov, Mikhail Berg, Larry K. McFarlane, Sally A. Flynn, Connor Ferrare, Richard Hostetler, Chris BE Picard, RH Schafer, K Comeron, A Kassianov, E Mertens, CJ TI The 3D Radiative Effects of Clouds in Aerosol Retrieval: Can we Remove Them? SO REMOTE SENSING OF CLOUDS AND THE ATMOSPHERE XIV SE Proceedings of SPIE LA English DT Proceedings Paper CT 14th Conference on Remote Sensing of Clouds and the Atmosphere CY AUG 31-SEP 01, 2009 CL Berlin, GERMANY SP SPIE Europe DE Aerosol optical depth; cumulus clouds; multi-spectral reflectance; Monte Carlo radiative transfer calculations; aircraft observations ID SPECTRAL-RESOLUTION LIDAR; MODIS AB We outline a new method, called the ratio method, developed to retrieve aerosol optical depth (AOD) under broken cloud conditions and present validation results from sensitivity and case studies. Results of the sensitivity study demonstrate that the ratio method, which exploits ratios of reflectances in the visible spectral range, has the potential for accurate AOD retrievals under different observational conditions and random errors in input data. Also, we examine the performance of the ratio method using aircraft data collected during the Cloud and Land Surface Interaction Campaign (CLASIC) and the Cumulus Humilis Aerosol Processing Study (CHAPS). Results of the case study suggest that the ratio method has the ability to retrieve AOD from multi-spectral aircraft observations of the reflected solar radiation. C1 [Kassianov, Evgueni; Ovchinnikov, Mikhail; Berg, Larry K.; McFarlane, Sally A.; Flynn, Connor] Pacific NW Natl Lab, Richland, WA 99352 USA. [Ferrare, Richard; Hostetler, Chris] NASA Langley Res Ctr, Hampton, VA 23681 USA. RP Kassianov, E (reprint author), Pacific NW Natl Lab, Richland, WA 99352 USA. EM Evgueni.Kassianov@pnl.gov RI Berg, Larry/A-7468-2016 OI Berg, Larry/0000-0002-3362-9492 FU National Aeronautics and Space Administration ( NASA) through the Radiation Sciences Program; Office of Biological and Environmental Research ( OBER) of the U. S. Department of Energy ( DOE) as part of the Atmospheric Radiation Measurement ( ARM) Program; Atmospheric Science Program ( ASP); Battelle for the DOE [DE- AC0676RLO 1830]; OE, OBER and located at PNNL FX This work was supported by the National Aeronautics and Space Administration ( NASA) through the Radiation Sciences Program and the Office of Biological and Environmental Research ( OBER) of the U. S. Department of Energy ( DOE) as part of the Atmospheric Radiation Measurement ( ARM) Program and Atmospheric Science Program ( ASP). The Pacific Northwest National Laboratory ( PNNL) is operated by Battelle for the DOE under contract DE- AC0676RLO 1830. This research was performed in part using the Molecular Science Computing Facility ( MSCF) in the Environmental Molecular Sciences Laboratory ( EMSL), a national scientific user facility sponsored by the U. S. DOE, OBER and located at PNNL. NR 14 TC 0 Z9 0 U1 0 U2 0 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 978-0-8194-7780-4 J9 PROC SPIE PY 2009 VL 7475 AR UNSP 74750I DI 10.1117/12.830179 PG 7 WC Meteorology & Atmospheric Sciences; Remote Sensing; Optics SC Meteorology & Atmospheric Sciences; Remote Sensing; Optics GA BA7EJ UT WOS:000337499500013 ER PT S AU Krueger, A Yang, K Krotkov, N AF Krueger, Arlin Yang, Kai Krotkov, Nickolay BE Picard, RH Schafer, K Comeron, A Kassianov, E Mertens, CJ TI Enhanced monitoring of sulfur dioxide sources with hyperspectral UV sensors SO REMOTE SENSING OF CLOUDS AND THE ATMOSPHERE XIV SE Proceedings of SPIE LA English DT Proceedings Paper CT 14th Conference on Remote Sensing of Clouds and the Atmosphere CY AUG 31-SEP 01, 2009 CL Berlin, GERMANY SP SPIE Europe DE Hyperspectral; Remote Sensing; UV spectrometer; Sulfur Dioxide; Volcanic emissions; Air quality; Aviation hazards ID OZONE MAPPING SPECTROMETER; EL-CHICHON; INSTRUMENT; GOME; TOMS AB Sulfur dioxide, a short-lived atmospheric constituent, is oxidized to sulfate aerosols, a climate agent. Main sources are volcanoes, smelters, and fossil fuel combustion. Satellite monitoring of SO2 began with TOMS data in 1978 that detected volcanic eruption clouds. Hyperspectral instruments, like OMI and GOME, have a twenty-fold improvement in sensitivity. Degassing volcanoes, smelters, and large power plants are now monitored for a database of SO2 emission to the atmosphere. SO2 is a distinctive marker for volcanic ash clouds, a hazard to aircraft. C1 [Krueger, Arlin] Univ Maryland Baltimore Cty, Joint Ctr Earth Sci Technol, Baltimore, MD 21250 USA. [Yang, Kai; Krotkov, Nickolay] Univ Maryland Baltimore Cty, Goddard Earth Sci & Technol Ctr, Baltimore, MD 21250 USA. RP Krueger, A (reprint author), Univ Maryland Baltimore Cty, Joint Ctr Earth Sci Technol, Baltimore, MD 21250 USA. EM akrueger@umbc.edu RI Krotkov, Nickolay/E-1541-2012 OI Krotkov, Nickolay/0000-0001-6170-6750 FU NASA TOMS and OMI Science Teams; NASA Applications Program Cooperative Agreement Grant [NNS06AA05G] FX This work was supported by NASA TOMS and OMI Science Teams and by the NASA Applications Program Cooperative Agreement Grant NNS06AA05G (NASA research volcanic emissions data for Aviation Hazards). In-kind support has been provided by NOAA/NESDIS and USGS. NR 15 TC 0 Z9 0 U1 1 U2 1 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 978-0-8194-7780-4 J9 PROC SPIE PY 2009 VL 7475 AR UNSP 74750Y DI 10.1117/12.830142 PG 9 WC Meteorology & Atmospheric Sciences; Remote Sensing; Optics SC Meteorology & Atmospheric Sciences; Remote Sensing; Optics GA BA7EJ UT WOS:000337499500026 ER PT S AU Mertens, CJ Xu, X Fernandez, JR Bilitza, D Russell, JM Mlynczak, MG AF Mertens, C. J. Xu, X. Fernandez, J. R. Bilitza, D. Russell, J. M., III Mlynczak, M. G. BE Picard, RH Schafer, K Comeron, A Kassianov, E Mertens, CJ TI Development of a Geomagnetic Storm Correction to the International Reference Ionosphere E-Region Electron Densities Using TIMED/SABER Observations SO REMOTE SENSING OF CLOUDS AND THE ATMOSPHERE XIV SE Proceedings of SPIE LA English DT Proceedings Paper CT 14th Conference on Remote Sensing of Clouds and the Atmosphere CY AUG 31-SEP 01, 2009 CL Berlin, GERMANY SP SPIE Europe ID KINETIC TEMPERATURE; CORRECTION MODEL; CARBON-DIOXIDE; EMISSION; IRI2000 AB Auroral infrared emission observed from the TIMED/SABER broadband 4.3 um channel is used to develop an empirical geomagnetic storm correction to the International Reference Ionosphere (IRI) E-region electron densities. The observation-based proxy used to develop the storm model is SABER-derived NO+(v) 4.3 um volume emission rates (VER). A correction factor is defined as the ratio of storm-time NO+(v) 4.3 um VER to a quiet-time climatological averaged NO+(v) 4.3 um VER, which is linearly fit to available geomagnetic activity indices. The initial version of the E-region storm model, called STORM-E, is most applicable within the auroral oval region. The STORM-E predictions of E-region electron densities are compared to incoherent scatter radar electron density measurements during the Halloween 2003 storm events. Future STORM-E updates will extend the model outside the auroral oval. C1 [Mertens, C. J.; Fernandez, J. R.; Mlynczak, M. G.] NASA, Langley Res Ctr, Hampton, VA 23665 USA. [Xu, X.] SSAI Inc, Hampton, VA USA. [Bilitza, D.] George Mason Univ, Fairfax, VA 22030 USA. [Russell, J. M., III] Hampton Univ, Hampton, VA 23668 USA. RP Mertens, CJ (reprint author), NASA, Langley Res Ctr, Hampton, VA 23665 USA. FU National Aeronautics and Space Administration [NNH06DA001N] FX This material is based upon work supported by the National Aeronautics and Space Administration under grant NNH06DA001N issued through the Science Mission Directorate's Living With A Star Targeted Research and Technology Program. NR 14 TC 1 Z9 1 U1 0 U2 0 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 978-0-8194-7780-4 J9 PROC SPIE PY 2009 VL 7475 AR UNSP 747508 DI 10.1117/12.829976 PG 12 WC Meteorology & Atmospheric Sciences; Remote Sensing; Optics SC Meteorology & Atmospheric Sciences; Remote Sensing; Optics GA BA7EJ UT WOS:000337499500006 ER PT S AU Sano, I Mukai, S Mukai, M Holben, B Slutsker, I AF Sano, I. Mukai, S. Mukai, M. Holben, B. Slutsker, I. BE Picard, RH Schafer, K Comeron, A Kassianov, E Mertens, CJ TI Estimation algorithm for aerosol properties from CAI on GOSAT SO REMOTE SENSING OF CLOUDS AND THE ATMOSPHERE XIV SE Proceedings of SPIE LA English DT Proceedings Paper CT 14th Conference on Remote Sensing of Clouds and the Atmosphere CY AUG 31-SEP 01, 2009 CL Berlin, GERMANY SP SPIE Europe DE Aerosols; absorbing particles; GOSAT; CAI; GLI; MODIS; POLDER ID OPTICAL-PROPERTIES; DIELECTRIC-CONSTANT; LAND SURFACES; SMOKE AB Green house gases observational satellite (GOSAT) was successfully launched on 23 January in 2009 by JAXA. The satellite carries two sensors, Fourier Transform Spectrometer (FTS) and Cloud Aerosol Imager (CAI). The CAI has four observing wavelengths as 0.38, 0.67, 0.87 and 1.6 mu m. It is shown here that this CAI/0.38 mu m is a unique observing band among usual sensors as MODIS and so on, and it is useful to distinguish the aerosol characteristics of absorbing (e. g., biomass burning) or non-absorbing (e. g., sulfate). In other word, this work proposed a space based retrieval algorithm for atmospheric aerosols including estimation of the optical constant for biomass burning particles. Our algorithm aims to apply the combination use of near UV data with GOAT/CAI, the violet data with Aqua/MODIS and near-IR polarization data with PARASOL/POLDER. In practice the algorithm has been partly examined by using ADEOS-2 / GLI data. C1 [Sano, I.; Mukai, S.] Kinki Univ, Fac Sci & Technol, 3-4-1 Kowakae, Higashi Osaka 5778502, Japan. [Mukai, M.] Japan Aerosp Explorat Agcy, EORC, Tsukuba, Ibaraki 3058505, Japan. [Holben, B.; Slutsker, I.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Sano, I (reprint author), Kinki Univ, Fac Sci & Technol, 3-4-1 Kowakae, Higashi Osaka 5778502, Japan. FU GOSAT/CAI (NIES, Japan); GCOM-C/SGLI (JAXA, Japan); Ministry of Education, Culture, Sports, Science and Technology in Japan [21120509] FX The authors gratefully acknowledge the JAXA/EORC for GLI data processing. This work was supported in part by grant for GOSAT/CAI (NIES, Japan), GCOM-C/SGLI (JAXA, Japan), and by a Grant-in-Aid for Scientific Research from the Ministry of Education, Culture, Sports, Science and Technology in Japan (No. 21120509). NR 18 TC 0 Z9 0 U1 1 U2 1 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 978-0-8194-7780-4 J9 PROC SPIE PY 2009 VL 7475 AR UNSP 74751E DI 10.1117/12.830155 PG 8 WC Meteorology & Atmospheric Sciences; Remote Sensing; Optics SC Meteorology & Atmospheric Sciences; Remote Sensing; Optics GA BA7EJ UT WOS:000337499500040 ER PT S AU Szewczyk, ZP Priestley, KJ AF Szewczyk, Z. Peter Priestley, Kory J. BE Picard, RH Schafer, K Comeron, A Kassianov, E Mertens, CJ TI CERES (FM2) Field Campaigns of 2008 SO REMOTE SENSING OF CLOUDS AND THE ATMOSPHERE XIV SE Proceedings of SPIE LA English DT Proceedings Paper CT 14th Conference on Remote Sensing of Clouds and the Atmosphere CY AUG 31-SEP 01, 2009 CL Berlin, GERMANY SP SPIE Europe AB A Clouds and the Earth's Radiant Energy System instrument (FM2) on board the Terra satellite has been used in field campaigns to provide TOA radiance measurements. Using a special programmable azimuth plan scan (PAPS) mode, a scanner collects data over a specified Earth target or of a prescribed spatial orientation. This paper covers operational aspects of four field campaigns in which FM2 participated in 2008. These include the annual CERES/GERB comparison campaign carried out at the summer and winter solstices, an aerosol campaign over Beijing ran before, during and after Summer Olympics, calibration and validation of GERB radiances at the ground station in Alacante/Spain, and also a bi-weekly true long-track scan for comparison to true nadir instruments. C1 [Szewczyk, Z. Peter] SAIC, Hampton, VA 23666 USA. [Priestley, Kory J.] NASA, Langley Res Ctr, Hampton, VA 23681 USA. RP Szewczyk, ZP (reprint author), SAIC, Hampton, VA 23666 USA. EM z.peter.szewczyk@nasa.gov; kory.j.priestley@nasa.gov NR 12 TC 0 Z9 0 U1 0 U2 0 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 978-0-8194-7780-4 J9 PROC SPIE PY 2009 VL 7475 AR UNSP 74750E DI 10.1117/12.829854 PG 10 WC Meteorology & Atmospheric Sciences; Remote Sensing; Optics SC Meteorology & Atmospheric Sciences; Remote Sensing; Optics GA BA7EJ UT WOS:000337499500010 ER PT S AU Cantrell, JH AF Cantrell, John H. BE Thompson, DO Chimenti, DE TI NONDESTRUCTIVE EVALUATION OF METAL FATIGUE USING NONLINEAR ACOUSTICS SO REVIEW OF PROGRESS IN QUANTITATIVE NONDESTRUCTIVE EVALUATION, VOLS 28A AND 28B SE AIP Conference Proceedings LA English DT Proceedings Paper CT 35th Annual Review of Progress in Quantitative Nondestructive Evaluation CY JUL 20-25, 2008 CL Univ Chicago, Chicago, IL HO Univ Chicago DE Nonlinear Acoustics; Metal Fatigue; Microelastic-Plastic Nonlinearity; Dislocation Substructures ID WAVY SLIP METALS; HARMONIC-GENERATION; ULTRASONIC-WAVES; DAMAGE ACCUMULATION; SOLIDS AB Safe-life and damage-tolerant design philosophies of high performance structures have driven the development of various methods to evaluate nondestructively the accumulation of damage in such structures resulting from cyclic loading. Although many techniques have proven useful, none has been able to provide an unambiguous, quantitative assessment of damage accumulation at each stage of fatigue from the virgin state to fracture. A method based on nonlinear acoustics is shown to provide such a means to assess the state of metal fatigue. The salient features of an analytical model are presented of the microelastic-plastic nonlinearities resulting from the interaction of an acoustic wave with fatigue-generated dislocation substructures and cracks that predictably evolve during the metal fatigue process. The interaction is quantified by the material (acoustic) nonlinearity parameter beta extracted from acoustic harmonic generation measurements. The beta parameters typically increase monotonically by several hundred percent over the fatigue life of the metal, thus providing a unique measure of the state of fatigue. Application of the model to aluminum alloy 2024-T4 and 410Cb stainless steel specimens fatigued using different loading conditions yields good agreement between theory and experiment. Application of the model and measurement technique to the on-site inspection of steam turbine blades is discussed. C1 NASA, Langley Res Ctr, Hampton, VA 23681 USA. RP Cantrell, JH (reprint author), NASA, Langley Res Ctr, Mail Stop 231, Hampton, VA 23681 USA. NR 22 TC 5 Z9 5 U1 0 U2 3 PU AMER INST PHYSICS PI MELVILLE PA 2 HUNTINGTON QUADRANGLE, STE 1NO1, MELVILLE, NY 11747-4501 USA SN 0094-243X BN 978-0-7354-0629-2 J9 AIP CONF PROC PY 2009 VL 1096 BP 19 EP 32 PG 14 WC Materials Science, Characterization & Testing; Physics, Applied SC Materials Science; Physics GA BKO01 UT WOS:000268740800002 ER PT S AU Cantrell, JH AF Cantrell, John H. BE Thompson, DO Chimenti, DE TI ACOUSTIC RECTIFICATION IN DISPERSIVE MEDIA SO REVIEW OF PROGRESS IN QUANTITATIVE NONDESTRUCTIVE EVALUATION, VOLS 28A AND 28B SE AIP Conference Proceedings LA English DT Proceedings Paper CT 35th Annual Review of Progress in Quantitative Nondestructive Evaluation CY JUL 20-25, 2008 CL Univ Chicago, Chicago, IL HO Univ Chicago DE Radiation-Induced Static Pulses; Dispersive Media; Solitons ID RADIATION STRESS; SOLIDS AB It is shown that the shapes of acoustic radiation-induced static strain and displacement pulses (rectified acoustic pulses) are defined locally by the energy density of the generating waveform. Dispersive properties are introduced analytically by assuming that the rectified pulses are functionally dependent on a phase factor that includes both dispersive and nonlinear terms. The dispersion causes an evolutionary change in the shape of the energy density profile that leads to the generation of solitons experimentally observed in fused silica. C1 NASA, Langley Res Ctr, Hampton, VA 23681 USA. RP Cantrell, JH (reprint author), NASA, Langley Res Ctr, Mail Stop 231, Hampton, VA 23681 USA. NR 7 TC 0 Z9 0 U1 0 U2 1 PU AMER INST PHYSICS PI MELVILLE PA 2 HUNTINGTON QUADRANGLE, STE 1NO1, MELVILLE, NY 11747-4501 USA SN 0094-243X BN 978-0-7354-0629-2 J9 AIP CONF PROC PY 2009 VL 1096 BP 217 EP 223 PG 7 WC Materials Science, Characterization & Testing; Physics, Applied SC Materials Science; Physics GA BKO01 UT WOS:000268740800025 ER PT S AU Wincheski, B Simpson, J Hall, G AF Wincheski, Buzz Simpson, John Hall, George BE Thompson, DO Chimenti, DE TI EDDY CURRENT SYSTEM FOR DETECTION OF CRACKING BENEATH BRAIDING IN CORRUGATED METAL HOSE SO REVIEW OF PROGRESS IN QUANTITATIVE NONDESTRUCTIVE EVALUATION, VOLS 28A AND 28B SE AIP Conference Proceedings LA English DT Proceedings Paper CT 35th Annual Review of Progress in Quantitative Nondestructive Evaluation CY JUL 20-25, 2008 CL Univ Chicago, Chicago, IL HO Univ Chicago DE Eddy Current; Fatigue Crack; Corrugated Metal Hose; Flex Hose; Space Shuttle AB In this paper an eddy current system for the detection of partially-through-the-thickness cracks in corrugated metal hose is presented. Design criteria based upon the geometry and conductivity of the part are developed and applied to the fabrication of a prototype inspection system. Experimental data are used to highlight the capabilities of the system and an image processing technique is presented to improve flaw detection capabilities. A case study for detection of cracking damage in a space shuttle radiator retract flex hoses is also presented. C1 [Wincheski, Buzz] NASA, Langley Res Ctr, Hampton, VA 23681 USA. [Simpson, John] Lockheed Martin Space Operat, Hampton, VA 23681 USA. [Hall, George] George Washington Univ, Washington, DC 20052 USA. RP Wincheski, B (reprint author), NASA, Langley Res Ctr, Hampton, VA 23681 USA. NR 5 TC 0 Z9 0 U1 0 U2 0 PU AMER INST PHYSICS PI MELVILLE PA 2 HUNTINGTON QUADRANGLE, STE 1NO1, MELVILLE, NY 11747-4501 USA SN 0094-243X BN 978-0-7354-0629-2 J9 AIP CONF PROC PY 2009 VL 1096 BP 371 EP + PG 2 WC Materials Science, Characterization & Testing; Physics, Applied SC Materials Science; Physics GA BKO01 UT WOS:000268740800045 ER PT S AU Roth, DJ Tokars, RP Martin, RE Rauser, RW Aldrin, JC AF Roth, D. J. Tokars, R. P. Martin, R. E. Rauser, R. W. Aldrin, J. C. BE Thompson, DO Chimenti, DE TI ULTRASONIC PHASED ARRAY SIMULATIONS OF WELDED COMPONENTS AT NASA SO REVIEW OF PROGRESS IN QUANTITATIVE NONDESTRUCTIVE EVALUATION, VOLS 28A AND 28B SE AIP Conference Proceedings LA English DT Proceedings Paper CT 35th Annual Review of Progress in Quantitative Nondestructive Evaluation CY JUL 20-25, 2008 CL Univ Chicago, Chicago, IL HO Univ Chicago DE Nondestructive Evaluation; Computational Simulation; Ultrasonics; Weld; Modeling; Phased Array AB Comprehensive and accurate inspections of welded components have become of increasing importance as NASA develops new hardware such as Ares rocket segments for future exploration missions. Simulation and modeling will play an increasing role in the future for nondestructive evaluation in order to better understand the physics of the inspection process, to prove or disprove the feasibility for an inspection method or inspection scenario, for inspection optimization, for better understanding of experimental results, and for assessment of probability of detection. This study presents simulation and experimental results for an ultrasonic phased array inspection of a critical welded structure important for NASA future exploration vehicles. C1 [Roth, D. J.; Tokars, R. P.] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. [Rauser, R. W.] Univ Toledo, Toledo, OH USA. RP Roth, DJ (reprint author), NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. NR 13 TC 0 Z9 0 U1 0 U2 0 PU AMER INST PHYSICS PI MELVILLE PA 2 HUNTINGTON QUADRANGLE, STE 1NO1, MELVILLE, NY 11747-4501 USA SN 0094-243X BN 978-0-7354-0629-2 J9 AIP CONF PROC PY 2009 VL 1096 BP 1190 EP + PG 2 WC Materials Science, Characterization & Testing; Physics, Applied SC Materials Science; Physics GA BKO01 UT WOS:000268740800151 ER PT S AU Johnston, PH AF Johnston, P. H. BE Thompson, DO Chimenti, DE TI ADDRESSING THE LIMIT OF DETECTABILITY OF RESIDUAL OXIDE DISCONTINUITIES IN FRICTION STIR BUTT WELDS OF ALUMINUM USING PHASED ARRAY ULTRASOUND SO REVIEW OF PROGRESS IN QUANTITATIVE NONDESTRUCTIVE EVALUATION, VOLS 28A AND 28B SE AIP Conference Proceedings LA English DT Proceedings Paper CT 35th Annual Review of Progress in Quantitative Nondestructive Evaluation CY JUL 20-25, 2008 CL Univ Chicago, Chicago, IL HO Univ Chicago DE Ultrasonic NDE; Friction Stir Weld; Residual Oxide Discontinuity AB This activity seeks to estimate a theoretical upper bound of detectability for a layer of oxide embedded in a friction stir weld in aluminum. The oxide is theoretically modeled as an ideal planar layer of aluminum oxide, oriented normal to an interrogating ultrasound beam. Experimentally-measured grain scattering level is used to represent the practical noise floor. Echoes from naturally-occurring oxides will necessarily fall below this theoretical limit, and must be above the measurement noise to be potentially detectable. C1 NASA, Langley Res Ctr, Hampton, VA 23681 USA. RP Johnston, PH (reprint author), NASA, Langley Res Ctr, Hampton, VA 23681 USA. NR 3 TC 1 Z9 2 U1 0 U2 1 PU AMER INST PHYSICS PI MELVILLE PA 2 HUNTINGTON QUADRANGLE, STE 1NO1, MELVILLE, NY 11747-4501 USA SN 0094-243X BN 978-0-7354-0629-2 J9 AIP CONF PROC PY 2009 VL 1096 BP 1902 EP 1909 PG 8 WC Materials Science, Characterization & Testing; Physics, Applied SC Materials Science; Physics GA BKO01 UT WOS:000268740800243 ER PT J AU Keiser, GM Adams, M Bencze, WJ Brumley, RW Buchman, S Clarke, B Conklin, J DeBra, DB Dolphin, M Hipkins, DN Holmes, T Everitt, CWF Goebel, JH Gill, D Green, GB Heifetz, M Kolodziejczak, J Li, J Lipa, J Lockhart, JM Mester, JC Muhlfelder, B Ohshima, Y Parkinson, BW Salomon, M Shestople, P Silbergleit, AS Stahl, K Taber, MA Turneaure, JP Wang, S Worden, P AF Keiser, G. M. Adams, M. Bencze, W. J. Brumley, R. W. Buchman, S. Clarke, B. Conklin, J. DeBra, D. B. Dolphin, M. Hipkins, D. N. Holmes, T. Everitt, C. W. F. Goebel, J. H. Gill, D. Green, G. B. Heifetz, M. Kolodziejczak, J. Li, J. Lipa, J. Lockhart, J. M. Mester, J. C. Muhlfelder, B. Ohshima, Y. Parkinson, B. W. Salomon, M. Shestople, P. Silbergleit, A. S. Stahl, K. Taber, M. A. Turneaure, J. P. Wang, S. Worden, P. TI Gravity Probe B(*) SO RIVISTA DEL NUOVO CIMENTO LA English DT Article ID B RELATIVITY MISSION; GYROSCOPE; PERFORMANCE; SATELLITE; MOTION; ROTOR AB This paper describes the flight hardware. on-orbit operations. and preliminary data analysis for the Gravity Probe B satellite. C1 [Keiser, G. M.; Adams, M.; Bencze, W. J.; Brumley, R. W.; Buchman, S.; Clarke, B.; Conklin, J.; DeBra, D. B.; Dolphin, M.; Hipkins, D. N.; Holmes, T.; Everitt, C. W. F.; Goebel, J. H.; Gill, D.; Green, G. B.; Heifetz, M.; Li, J.; Lipa, J.; Mester, J. C.; Muhlfelder, B.; Ohshima, Y.; Parkinson, B. W.; Salomon, M.; Shestople, P.; Silbergleit, A. S.; Stahl, K.; Taber, M. A.; Turneaure, J. P.; Wang, S.; Worden, P.] Stanford Univ, WW Hansen Expt Phys Lab, Stanford, CA 94305 USA. [Kolodziejczak, J.] NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA. [Lockhart, J. M.] San Francisco State Univ, Dept Phys & Astron, San Francisco, CA 94132 USA. RP Keiser, GM (reprint author), Stanford Univ, WW Hansen Expt Phys Lab, Stanford, CA 94305 USA. NR 61 TC 8 Z9 8 U1 0 U2 1 PU SOC ITALIANA FISICA PI BOLOGNA PA VIA SARAGOZZA, 12, I-40123 BOLOGNA, ITALY SN 0393-697X EI 1826-9850 J9 RIV NUOVO CIMENTO JI Riv. Nuovo Cimento PY 2009 VL 32 IS 11 BP 555 EP 589 DI 10.1393/ncr/i2009-10049-y PG 35 WC Physics, Multidisciplinary SC Physics GA 544RS UT WOS:000273677400001 ER PT S AU Barringer, H Havelund, K Rydeheard, D Groce, A AF Barringer, Howard Havelund, Klaus Rydeheard, David Groce, Alex BE Bensalem, S Peled, DA TI Rule Systems for Runtime Verification: A Short Tutorial SO RUNTIME VERIFICATION SE Lecture Notes in Computer Science LA English DT Proceedings Paper CT 9th International Workshop on Runtime Verification CY JUN 26-28, 2009 CL Grenoble, FRANCE DE Runtime verification; rule systems; temporal logic; code instrumentation; log file analysis; Java; AspectJ; Python AB In this tutorial, we introduce two rule-based systems for on and off-line trace analysis, RULER and LOGSCOPE. RULER is a conditional rule-based system, which has a simple and easily implemented algorithm for effective runtime verification, and into which one can compile a wide range of temporal logics and other specification formalisms used for runtime verification. Specifications can be parameterized with data, or even with specifications, allowing for temporal logic combinators to be defined. We outline a number of simple syntactic extensions of core RULER that can lead to further conciseness of specification but still enabling easy and efficient implementation. RuleR is implemented in Java and we will demonstrate its ease of use in monitoring Java programs. LOGSCOPE is a derivation of RULER adding a simple very user-friendly temporal logic. It was developed in Python, specifically for Supporting testing of spacecraft flight software for NASA's next 2011 Mars mission MSL (Mars Science Laboratory). The system has been applied by test engineers to analysis of log files generated by running the flight software. Detailed logging is already part of the system design approach, and hence there is no added instrumentation overhead caused by this approach. While post-mortem log analysis prevents the autonomous reaction to problems possible with traditional runtime verification, it provides a powerful tool for test automation. A new system is being developed that integrates features from both RULER and LOGSCOPE. C1 [Barringer, Howard; Rydeheard, David] Univ Manchester, Sch Comp Sci, Oxford Rd, Manchester M13 9PL, Lancs, England. [Havelund, Klaus] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Groce, Alex] Oregon State Univ, Sch Elect Engn & Comp Sci, Corvallis, OR 97331 USA. RP Barringer, H (reprint author), Univ Manchester, Sch Comp Sci, Oxford Rd, Manchester M13 9PL, Lancs, England. EM Howard.Barringer@manchester.ac.uk; Klaus.Havelund@jpl.nasa.gov; David.Rydeheard@manchester.ac.uk; Alex@eecs.oregonstate.edu NR 21 TC 5 Z9 5 U1 0 U2 0 PU SPRINGER-VERLAG BERLIN PI BERLIN PA HEIDELBERGER PLATZ 3, D-14197 BERLIN, GERMANY SN 0302-9743 BN 978-3-642-04693-3 J9 LECT NOTES COMPUT SC PY 2009 VL 5779 BP 1 EP + PG 3 WC Computer Science, Hardware & Architecture; Computer Science, Theory & Methods SC Computer Science GA BMU92 UT WOS:000273623300001 ER PT S AU Tran, D Chien, S Rabideau, G Cichy, B AF Tran, Daniel Chien, Steve Rabideau, Gregg Cichy, Benjamin BE Barley, M Mouratidis, H Unruh, A Spears, D Scerri, P Massacci, F TI Safe Agents in Space: Preventing and Responding to Anomalies in the Autonomous Sciencecraft Experiment SO SAFETY AND SECURITY IN MULTIAGENT SYSTEMS: RESEARCH RESULTS FROM 2004-2006 SE Lecture Notes in Artificial Intelligence LA English DT Article; Book Chapter AB This paper describes the design of the Autonomous Sciencecraft Experiment, a software agent that has been running on-board the EO-1 spacecraft since 2003. The agent recognizes science events, retargets the spacecraft to respond to the science events, and reduces data downlink to only the highest value science data. The autonomous science agent was designed using a layered architectural approach with specific redundant safeguards to reduce the risk of an agent malfunction to the EO-1 spacecraft. The agent was designed to be "safe" by first preventing anomalies, then by automatically detecting and responding to them when possible. This paper describes elements of the design that increase the safety of the agent, several of the anomalies that occurred during the experiment, and how the agent responded to these anomalies. C1 [Tran, Daniel; Chien, Steve; Rabideau, Gregg; Cichy, Benjamin] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. RP Tran, D (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. EM Daniel.Tran@jpl.nasa.gov; Steve.Chien@jpl.nasa.gov; Gregg.Rabideau@jpl.nasa.gov; Benjamin.Cichy@jpl.nasa.gov NR 10 TC 0 Z9 0 U1 0 U2 1 PU SPRINGER-VERLAG BERLIN PI BERLIN PA HEIDELBERGER PLATZ 3, D-14197 BERLIN, GERMANY SN 0302-9743 BN 978-3-642-04878-4 J9 LECT NOTES ARTIF INT PY 2009 VL 4324 BP 147 EP 161 D2 10.1007/978-3-642-04879-1 PG 15 WC Computer Science, Artificial Intelligence; Computer Science, Theory & Methods SC Computer Science GA BLW07 UT WOS:000271196900011 ER PT S AU Martin, C Schreckenghost, D Bonasso, P AF Martin, Cheryl Schreckenghost, Debra Bonasso, Pete BE Barley, M Mouratidis, H Unruh, A Spears, D Scerri, P Massacci, F TI Command and Authorization Services for Multiple Humans Interacting with a Software Control Agent for Advanced Life Support SO SAFETY AND SECURITY IN MULTIAGENT SYSTEMS: RESEARCH RESULTS FROM 2004-2006 SE Lecture Notes in Artificial Intelligence LA English DT Article; Book Chapter ID INTELLIGENT CONTROL; SPACE AB This paper describes current work developing command and authorization services to support the coordination of multiple humans and an autonomous control agent working on the same underlying advanced life support system. The primary goal of these services is to prevent unknowing or accidental conflicts from arising as a result of issuing commands or taking action on the system. Avoiding such conflicts minimizes the risk of interfering with the work of another agent or putting the system into an unsafe operating state. This paper provides an overview of the advanced life support system at NASA to which this work has been applied and then discusses details for authorization, overrides, and system reconfiguration for commanding. C1 [Martin, Cheryl] Univ Texas Austin, Appl Res Labs, Austin, TX 78713 USA. [Schreckenghost, Debra; Bonasso, Pete] NASA, Lyndon B Johnson Space Ctr, TRACLabs, Houston, TX 77058 USA. RP Martin, C (reprint author), Univ Texas Austin, Appl Res Labs, POB 8029, Austin, TX 78713 USA. EM cmartin@arlut.utexas.edu; ghost@ieee.org; r.p.bonasso@jsc.nasa.gov NR 29 TC 0 Z9 0 U1 0 U2 0 PU SPRINGER-VERLAG BERLIN PI BERLIN PA HEIDELBERGER PLATZ 3, D-14197 BERLIN, GERMANY SN 0302-9743 BN 978-3-642-04878-4 J9 LECT NOTES ARTIF INT PY 2009 VL 4324 BP 225 EP 240 D2 10.1007/978-3-642-04879-1 PG 16 WC Computer Science, Artificial Intelligence; Computer Science, Theory & Methods SC Computer Science GA BLW07 UT WOS:000271196900016 ER PT J AU Marshall, YY AF Marshall, Yolanda Y. BE Musgrave, GE Larsen, AM Sgobba, T TI Introduction to Space Safety SO SAFETY DESIGN FOR SPACE SYSTEMS LA English DT Editorial Material; Book Chapter C1 NASA, Safety & Mission Assurance Directorate, Johnson Space Ctr, Houston, TX USA. RP Marshall, YY (reprint author), NASA, Safety & Mission Assurance Directorate, Johnson Space Ctr, Houston, TX USA. NR 2 TC 1 Z9 1 U1 0 U2 0 PU ELSEVIER BUTTERWORTH-HEINEMANN PI BURLINGTON PA 30 CORPORATE DRIVE, STE 400, BURLINGTON, MA 01803 USA BN 978-0-08-055922-3 PY 2009 BP 1 EP 5 DI 10.1016/B978-0-7506-8580-1.00001-4 PG 5 WC Engineering, Aerospace SC Engineering GA BGC95 UT WOS:000322363700003 ER PT B AU O'Connor, B AF O'Connor, Bryan BE Musgrave, GE Larsen, AM Sgobba, T TI Safety Design for Space Systems Preface SO SAFETY DESIGN FOR SPACE SYSTEMS LA English DT Editorial Material; Book Chapter C1 NASA, Washington, DC 20546 USA. RP O'Connor, B (reprint author), NASA, Washington, DC 20546 USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU ELSEVIER BUTTERWORTH-HEINEMANN PI BURLINGTON PA 30 CORPORATE DRIVE, STE 400, BURLINGTON, MA 01803 USA BN 978-0-08-055922-3 PY 2009 BP XXIII EP XXIII DI 10.1016/B978-0-7506-8580-1.00031-2 PG 1 WC Engineering, Aerospace SC Engineering GA BGC95 UT WOS:000322363700001 ER PT B AU Musgrave, GE AF Musgrave, Gary Eugene BE Musgrave, GE Larsen, AM Sgobba, T TI Safety Design for Space Systems Introduction SO SAFETY DESIGN FOR SPACE SYSTEMS LA English DT Editorial Material; Book Chapter C1 [Musgrave, Gary Eugene] NASA, NASA Payload Safety Review Panel, Johnson Space Ctr, Houston, TX USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU ELSEVIER BUTTERWORTH-HEINEMANN PI BURLINGTON PA 30 CORPORATE DRIVE, STE 400, BURLINGTON, MA 01803 USA BN 978-0-08-055922-3 PY 2009 BP XXV EP XXV DI 10.1016/B978-0-7506-8580-1.00032-4 PG 1 WC Engineering, Aerospace SC Engineering GA BGC95 UT WOS:000322363700002 ER PT J AU Sgobba, T Larsen, AM Musgrave, GE AF Sgobba, Tommaso Larsen, Axel M. (Skip), Jr. Musgrave, Gary E. BE Musgrave, GE Larsen, AM Sgobba, T TI Basic Principles of Space Safety SO SAFETY DESIGN FOR SPACE SYSTEMS LA English DT Article; Book Chapter C1 [Sgobba, Tommaso] European Space Agcy, European Space Res & Technol Ctr, Independent Flight Safety Off, NL-2200 AG Noordwijk, Netherlands. [Larsen, Axel M. (Skip), Jr.; Musgrave, Gary E.] NASA, NASA Payload Safety Review Panel, Johnson Space Ctr, Houston, TX USA. RP Sgobba, T (reprint author), European Space Agcy, European Space Res & Technol Ctr, Independent Flight Safety Off, NL-2200 AG Noordwijk, Netherlands. NR 5 TC 1 Z9 1 U1 0 U2 0 PU ELSEVIER BUTTERWORTH-HEINEMANN PI BURLINGTON PA 30 CORPORATE DRIVE, STE 400, BURLINGTON, MA 01803 USA BN 978-0-08-055922-3 PY 2009 BP 163 EP 174 DI 10.1016/B978-0-7506-8580-1.00004-X PG 12 WC Engineering, Aerospace SC Engineering GA BGC95 UT WOS:000322363700006 ER PT B AU Prokhorov, KS AF Prokhorov, Kimberlee S. BE Musgrave, GE Larsen, AM Sgobba, T TI Life Support Systems Safety SO SAFETY DESIGN FOR SPACE SYSTEMS LA English DT Article; Book Chapter C1 NASA, ISS Common Environm Team, Johnson Space Ctr, Houston, TX USA. RP Prokhorov, KS (reprint author), NASA, ISS Common Environm Team, Johnson Space Ctr, Houston, TX USA. NR 42 TC 0 Z9 0 U1 0 U2 0 PU ELSEVIER BUTTERWORTH-HEINEMANN PI BURLINGTON PA 30 CORPORATE DRIVE, STE 400, BURLINGTON, MA 01803 USA BN 978-0-08-055922-3 PY 2009 BP 185 EP 224 DI 10.1016/B978-0-7506-8580-1.00006-3 PG 40 WC Engineering, Aerospace SC Engineering GA BGC95 UT WOS:000322363700008 ER PT B AU Goodman, JR Grosveld, FW AF Goodman, Jerry R. Grosveld, Ferdinand W. BE Musgrave, GE Larsen, AM Sgobba, T TI Noise Control Design SO SAFETY DESIGN FOR SPACE SYSTEMS LA English DT Article; Book Chapter C1 [Goodman, Jerry R.] NASA, Acoust Working Grp, Houston, TX USA. [Goodman, Jerry R.] NASA, Johnson Space Ctr, Houston, TX USA. [Grosveld, Ferdinand W.] NASA Langley Res Ctr, Acoust & Fluid Mech Lockheed Martin Mission Serv, Houston, TX USA. [Grosveld, Ferdinand W.] Univ Kansas, Lawrence, KS 66045 USA. [Grosveld, Ferdinand W.] Old Dominion Univ, Norfolk, VA 23529 USA. RP Goodman, JR (reprint author), NASA, Johnson Space Ctr, Houston, TX USA. NR 20 TC 0 Z9 0 U1 0 U2 0 PU ELSEVIER BUTTERWORTH-HEINEMANN PI BURLINGTON PA 30 CORPORATE DRIVE, STE 400, BURLINGTON, MA 01803 USA BN 978-0-08-055922-3 PY 2009 BP 341 EP 357 DI 10.1016/B978-0-7506-8580-1.00011-7 PG 17 WC Engineering, Aerospace SC Engineering GA BGC95 UT WOS:000322363700013 ER PT B AU Pedley, MD AF Pedley, Michael D. BE Musgrave, GE Larsen, AM Sgobba, T TI Materials Safety SO SAFETY DESIGN FOR SPACE SYSTEMS LA English DT Article; Book Chapter C1 NASA, Mat & Proc Branch, Johnson Space Ctr, Houston, TX USA. RP Pedley, MD (reprint author), NASA, Mat & Proc Branch, Johnson Space Ctr, Houston, TX USA. NR 20 TC 0 Z9 0 U1 0 U2 0 PU ELSEVIER BUTTERWORTH-HEINEMANN PI BURLINGTON PA 30 CORPORATE DRIVE, STE 400, BURLINGTON, MA 01803 USA BN 978-0-08-055922-3 PY 2009 BP 359 EP 374 DI 10.1016/B978-0-7506-8580-1.00012-9 PG 16 WC Engineering, Aerospace SC Engineering GA BGC95 UT WOS:000322363700014 ER PT B AU Pedley, MD AF Pedley, Michael D. BE Musgrave, GE Larsen, AM Sgobba, T TI Oxygen Systems Safety SO SAFETY DESIGN FOR SPACE SYSTEMS LA English DT Article; Book Chapter C1 NASA, Mat & Proc Branch, Johnson Space Ctr, Houston, TX USA. RP Pedley, MD (reprint author), NASA, Mat & Proc Branch, Johnson Space Ctr, Houston, TX USA. NR 22 TC 0 Z9 0 U1 0 U2 0 PU ELSEVIER BUTTERWORTH-HEINEMANN PI BURLINGTON PA 30 CORPORATE DRIVE, STE 400, BURLINGTON, MA 01803 USA BN 978-0-08-055922-3 PY 2009 BP 375 EP 402 DI 10.1016/B978-0-7506-8580-1.00013-0 PG 28 WC Engineering, Aerospace SC Engineering GA BGC95 UT WOS:000322363700015 ER PT B AU Tadlock, DE AF Tadlock, David E. BE Musgrave, GE Larsen, AM Sgobba, T TI Avionics Safety SO SAFETY DESIGN FOR SPACE SYSTEMS LA English DT Article; Book Chapter C1 [Tadlock, David E.] NASA, Operat Space Syst Support Off, Johnson Space Ctr, Houston, TX USA. NR 25 TC 0 Z9 0 U1 0 U2 0 PU ELSEVIER BUTTERWORTH-HEINEMANN PI BURLINGTON PA 30 CORPORATE DRIVE, STE 400, BURLINGTON, MA 01803 USA BN 978-0-08-055922-3 PY 2009 BP 403 EP 474 DI 10.1016/B978-0-7506-8580-1.00014-2 PG 72 WC Engineering, Aerospace SC Engineering GA BGC95 UT WOS:000322363700016 ER PT J AU Leveson, NG Weiss, KA AF Leveson, Nancy G. Weiss, Kathryn Anne BE Musgrave, GE Larsen, AM Sgobba, T TI Software System Safety SO SAFETY DESIGN FOR SPACE SYSTEMS LA English DT Article; Book Chapter C1 [Leveson, Nancy G.] MIT, Boston, MA USA. [Weiss, Kathryn Anne] CALTECH, NASA Jet Prop Lab, Flight Software & Data Syst Sect, Pasadena, CA 91125 USA. RP Leveson, NG (reprint author), MIT, Boston, MA USA. NR 32 TC 0 Z9 0 U1 0 U2 0 PU ELSEVIER BUTTERWORTH-HEINEMANN PI BURLINGTON PA 30 CORPORATE DRIVE, STE 400, BURLINGTON, MA 01803 USA BN 978-0-08-055922-3 PY 2009 BP 475 EP 505 DI 10.1016/B978-0-7506-8580-1.00015-4 PG 31 WC Engineering, Aerospace SC Engineering GA BGC95 UT WOS:000322363700017 ER PT J AU Jeevarajan, JA AF Jeevarajan, Judith A. BE Musgrave, GE Larsen, AM Sgobba, T TI Battery Safety SO SAFETY DESIGN FOR SPACE SYSTEMS LA English DT Article; Book Chapter ID LITHIUM-ION BATTERIES; CELLS; MECHANISMS; VOLTAGE C1 NASA, Power Syst Branch, Johnson Space Ctr, Houston, TX USA. RP Jeevarajan, JA (reprint author), NASA, Power Syst Branch, Johnson Space Ctr, Houston, TX USA. NR 57 TC 1 Z9 1 U1 0 U2 1 PU ELSEVIER BUTTERWORTH-HEINEMANN PI BURLINGTON PA 30 CORPORATE DRIVE, STE 400, BURLINGTON, MA 01803 USA BN 978-0-08-055922-3 PY 2009 BP 507 EP 548 DI 10.1016/B978-0-7506-8580-1.00016-6 PG 42 WC Engineering, Aerospace SC Engineering GA BGC95 UT WOS:000322363700018 ER PT B AU Moreland, DW AF Moreland, Dean W. BE Musgrave, GE Larsen, AM Sgobba, T TI Mechanical Systems Safety SO SAFETY DESIGN FOR SPACE SYSTEMS LA English DT Article; Book Chapter C1 NASA, Payload Safety Review Panel, Johnson Space Ctr, Houston, TX USA. RP Moreland, DW (reprint author), NASA, Payload Safety Review Panel, Johnson Space Ctr, Houston, TX USA. NR 28 TC 0 Z9 0 U1 0 U2 0 PU ELSEVIER BUTTERWORTH-HEINEMANN PI BURLINGTON PA 30 CORPORATE DRIVE, STE 400, BURLINGTON, MA 01803 USA BN 978-0-08-055922-3 PY 2009 BP 549 EP 606 DI 10.1016/B978-0-7506-8580-1.00017-8 PG 58 WC Engineering, Aerospace SC Engineering GA BGC95 UT WOS:000322363700019 ER PT B AU Baumer, GJ AF Baumer, Gregg John BE Musgrave, GE Larsen, AM Sgobba, T TI Failure Tolerance Design SO SAFETY DESIGN FOR SPACE SYSTEMS LA English DT Article; Book Chapter C1 [Baumer, Gregg John] NASA, Int Space Stn Safety Review Panel, Johnson Space Ctr, Houston, TX USA. NR 3 TC 0 Z9 0 U1 0 U2 0 PU ELSEVIER BUTTERWORTH-HEINEMANN PI BURLINGTON PA 30 CORPORATE DRIVE, STE 400, BURLINGTON, MA 01803 USA BN 978-0-08-055922-3 PY 2009 BP 653 EP 660 DI 10.1016/B978-0-7506-8580-1.00019-1 PG 8 WC Engineering, Aerospace SC Engineering GA BGC95 UT WOS:000322363700021 ER PT B AU Van Tassel, KE AF Van Tassel, Keith E. BE Musgrave, GE Larsen, AM Sgobba, T TI Pyrotechnic Safety SO SAFETY DESIGN FOR SPACE SYSTEMS LA English DT Article; Book Chapter C1 NASA, Johnson Space Ctr, Houston, TX USA. RP Van Tassel, KE (reprint author), NASA, Johnson Space Ctr, Houston, TX USA. NR 3 TC 0 Z9 0 U1 0 U2 0 PU ELSEVIER BUTTERWORTH-HEINEMANN PI BURLINGTON PA 30 CORPORATE DRIVE, STE 400, BURLINGTON, MA 01803 USA BN 978-0-08-055922-3 PY 2009 BP 695 EP 704 DI 10.1016/B978-0-7506-8580-1.00021-X PG 10 WC Engineering, Aerospace SC Engineering GA BGC95 UT WOS:000322363700023 ER PT B AU Hornyak, D AF Hornyak, David BE Musgrave, GE Larsen, AM Sgobba, T TI Emergency, Caution, and Warning System SO SAFETY DESIGN FOR SPACE SYSTEMS LA English DT Article; Book Chapter C1 NASA, Johnson Space Ctr, Houston, TX USA. RP Hornyak, D (reprint author), NASA, Johnson Space Ctr, Houston, TX USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU ELSEVIER BUTTERWORTH-HEINEMANN PI BURLINGTON PA 30 CORPORATE DRIVE, STE 400, BURLINGTON, MA 01803 USA BN 978-0-08-055922-3 PY 2009 BP 725 EP 732 DI 10.1016/B978-0-7506-8580-1.00023-3 PG 8 WC Engineering, Aerospace SC Engineering GA BGC95 UT WOS:000322363700025 ER PT B AU Victor, JM AF Victor, Joe M. BE Musgrave, GE Larsen, AM Sgobba, T TI Laser Safety SO SAFETY DESIGN FOR SPACE SYSTEMS LA English DT Article; Book Chapter C1 NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. RP Victor, JM (reprint author), NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. NR 6 TC 0 Z9 0 U1 0 U2 0 PU ELSEVIER BUTTERWORTH-HEINEMANN PI BURLINGTON PA 30 CORPORATE DRIVE, STE 400, BURLINGTON, MA 01803 USA BN 978-0-08-055922-3 PY 2009 BP 733 EP 744 DI 10.1016/B978-0-7506-8580-1.00024-5 PG 12 WC Engineering, Aerospace SC Engineering GA BGC95 UT WOS:000322363700026 ER PT B AU Kirkpatrick, P Palo, T AF Kirkpatrick, Paul Palo, Thomas BE Musgrave, GE Larsen, AM Sgobba, T TI Safety Considerations for the Ground Environment SO SAFETY DESIGN FOR SPACE SYSTEMS LA English DT Article; Book Chapter C1 [Kirkpatrick, Paul] Ground Safety Review Panel, Kennedy Space Ctr, FL USA. [Kirkpatrick, Paul; Palo, Thomas] NASA, Kennedy Space Ctr, FL USA. RP Kirkpatrick, P (reprint author), Ground Safety Review Panel, Kennedy Space Ctr, FL USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU ELSEVIER BUTTERWORTH-HEINEMANN PI BURLINGTON PA 30 CORPORATE DRIVE, STE 400, BURLINGTON, MA 01803 USA BN 978-0-08-055922-3 PY 2009 BP 817 EP 828 DI 10.1016/B978-0-7506-8580-1.00026-9 PG 12 WC Engineering, Aerospace SC Engineering GA BGC95 UT WOS:000322363700028 ER PT J AU Ruff, GA Urban, DL Pedley, MD Johnson, PT AF Ruff, Gary A. Urban, David L. Pedley, Michael D. Johnson, Paul T. BE Musgrave, GE Larsen, AM Sgobba, T TI Fire Safety SO SAFETY DESIGN FOR SPACE SYSTEMS LA English DT Article; Book Chapter ID JET DIFFUSION FLAMES; LOW-VELOCITY FLOWS; PILOTED IGNITION; CARBON-DIOXIDE; MICROGRAVITY; COMBUSTION; GRAVITY; SPREAD; FUELS; SMOKE C1 [Ruff, Gary A.] NASA, Adv Capabil Project Off, Glenn Res Ctr, Cleveland, OH USA. [Urban, David L.] NASA, Combust & Reacting Syst Branch, Space Proc & Experiments Div, Glenn Res Ctr, Cleveland, OH USA. [Pedley, Michael D.] NASA, Mat & Proc Branch, Lyndon B Johnson Space Ctr, Houston, TX USA. [Johnson, Paul T.] Boeing Co, Safety & Reliabil, Huntsville, AL USA. RP Ruff, GA (reprint author), NASA, Adv Capabil Project Off, Glenn Res Ctr, Cleveland, OH USA. NR 104 TC 1 Z9 1 U1 0 U2 0 PU ELSEVIER BUTTERWORTH-HEINEMANN PI BURLINGTON PA 30 CORPORATE DRIVE, STE 400, BURLINGTON, MA 01803 USA BN 978-0-08-055922-3 PY 2009 BP 829 EP 883 DI 10.1016/B978-0-7506-8580-1.00027-0 PG 55 WC Engineering, Aerospace SC Engineering GA BGC95 UT WOS:000322363700029 ER PT B AU Baumer, GJ AF Baumer, Gregg John BE Musgrave, GE Larsen, AM Sgobba, T TI Safe Without Services Design SO SAFETY DESIGN FOR SPACE SYSTEMS LA English DT Article; Book Chapter C1 [Baumer, Gregg John] Int Space Stn Safety Review Panel, Houston, TX USA. [Baumer, Gregg John] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. RP Baumer, GJ (reprint author), NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU ELSEVIER BUTTERWORTH-HEINEMANN PI BURLINGTON PA 30 CORPORATE DRIVE, STE 400, BURLINGTON, MA 01803 USA BN 978-0-08-055922-3 PY 2009 BP 885 EP 888 DI 10.1016/B978-0-7506-8580-1.00028-2 PG 4 WC Engineering, Aerospace SC Engineering GA BGC95 UT WOS:000322363700030 ER PT B AU Stamatelatos, MG Vesely, WE Prassinos, PG AF Stamatelatos, Michael G. Vesely, William E. Prassinos, Peter G. BE Musgrave, GE Larsen, AM Sgobba, T TI Probabilistic Risk Assessment with Emphasis on Design SO SAFETY DESIGN FOR SPACE SYSTEMS LA English DT Article; Book Chapter C1 [Stamatelatos, Michael G.; Vesely, William E.; Prassinos, Peter G.] NASA, Off Safety & Mission Assurance, Washington, DC 20546 USA. RP Stamatelatos, MG (reprint author), NASA, Off Safety & Mission Assurance, Washington, DC 20546 USA. NR 3 TC 0 Z9 0 U1 0 U2 0 PU ELSEVIER BUTTERWORTH-HEINEMANN PI BURLINGTON PA 30 CORPORATE DRIVE, STE 400, BURLINGTON, MA 01803 USA BN 978-0-08-055922-3 PY 2009 BP 889 EP 911 DI 10.1016/B978-0-7506-8580-1.00029-4 PG 23 WC Engineering, Aerospace SC Engineering GA BGC95 UT WOS:000322363700031 ER PT B AU Russell, M Lecakes, GD Mandayam, S Morris, JA Turowski, M Schmalzel, JL AF Russell, Michael Lecakes, George D., Jr. Mandayam, Shreekanth Morris, Jonathan A. Turowski, Mark Schmalzel, John L. GP IEEE TI Acquisition, Interfacing and Analysis of Sensor Measurements in a VR Environment for Integrated Systems Health Management in Rocket Engine Tests SO SAS 2009 - IEEE SENSORS APPLICATIONS SYMPOSIUM, PROCEEDINGS LA English DT Proceedings Paper CT 4th IEEE Sensors Applications Symposium CY FEB 17-19, 2009 CL New Orleans, LA SP IEEE Instrumentat & Measurement Soc DE Data Acquisition; Network Interface; Failure Analysis; Virtual Reality; Visualization AB This paper presents our ongoing work in the area of using virtual reality (VR) environments for the integrated systems health management of complex test environments, such as those found in a rocket engine test stand. Specifically, the paper focuses on the design, development and implementation of a hardware-software framework for acquiring, interfacing, integrating and analyzing multiple sensor measurements for display inside of a VR environment. IEEE and OSA-CBM standards are used to design the acquisition and interface methods. Commercial off-the-shelf software is used for analysis and integration. Results demonstrating the application of our method to a rocket engine test stand are presented. C1 [Russell, Michael; Lecakes, George D., Jr.; Mandayam, Shreekanth] Rowan Univ, Dept Elect & Comp Engn, Glassboro, NJ 08028 USA. [Morris, Jonathan A.; Turowski, Mark; Schmalzel, John L.] NASA, Stennis Space Ctr, Bay St Louis, MS 39529 USA. RP Russell, M (reprint author), Rowan Univ, Dept Elect & Comp Engn, Glassboro, NJ 08028 USA. NR 6 TC 0 Z9 0 U1 0 U2 0 PU IEEE PI NEW YORK PA 345 E 47TH ST, NEW YORK, NY 10017 USA BN 978-1-4244-2786-4 PY 2009 BP 128 EP + DI 10.1109/SAS.2009.4801792 PG 2 WC Engineering, Electrical & Electronic; Instruments & Instrumentation; Remote Sensing SC Engineering; Instruments & Instrumentation; Remote Sensing GA BKL67 UT WOS:000268444000027 ER PT B AU Lecakes, GD Russell, M Mandayam, S Morris, JA Schmalzel, JL AF Lecakes, George D., Jr. Russell, Michael Mandayam, Shreekanth Morris, Jonathan A. Schmalzel, John L. GP IEEE TI Visualization of Multiple Sensor Measurements in a VR Environment for Integrated Systems Health Management in Rocket Engine Tests SO SAS 2009 - IEEE SENSORS APPLICATIONS SYMPOSIUM, PROCEEDINGS LA English DT Proceedings Paper CT 4th IEEE Sensors Applications Symposium CY FEB 17-19, 2009 CL New Orleans, LA SP IEEE Instrumentat & Measurement Soc DE Virtual Reality; Visualization; Virtual Instrumentation; Condition Based Monitoring; Graphical User Interface; Modeling and Simulation AB This paper presents our continuing work in the area of using virtual reality (VR) environments for the integrated systems health management of complex test environments, such as those found in a rocket engine test stand. Specifically, the paper focuses on the design and development of a software framework for integrating and displaying multiple sensor measurements. Various forms of data are displayed inside the VR environment in conjunction with the associated graphics which correspond to the physical structure of the test-stand (piping, valves, sensors, etc.). Results demonstrating the application of our method for visualizing scalar, vector and system-state data are presented. C1 [Lecakes, George D., Jr.; Russell, Michael; Mandayam, Shreekanth] Rowan Univ, Dept Elect & Comp Engn, Glassboro, NJ 08028 USA. [Morris, Jonathan A.; Schmalzel, John L.] NASA, Stennis Space Ctr, Bay St Louis, MS 39529 USA. RP Lecakes, GD (reprint author), Rowan Univ, Dept Elect & Comp Engn, Glassboro, NJ 08028 USA. FU NASA, Space Center [NNS06AC08P, NNX07AO92H] FX This work is supported by NASA John C. Stennis Space Center under Order No. NNS06AC08P and Grant No. NNX07AO92H. NR 8 TC 1 Z9 1 U1 0 U2 0 PU IEEE PI NEW YORK PA 345 E 47TH ST, NEW YORK, NY 10017 USA BN 978-1-4244-2786-4 PY 2009 BP 132 EP + DI 10.1109/SAS.2009.4801793 PG 2 WC Engineering, Electrical & Electronic; Instruments & Instrumentation; Remote Sensing SC Engineering; Instruments & Instrumentation; Remote Sensing GA BKL67 UT WOS:000268444000028 ER PT B AU Wang, CT Woodard, SE Taylor, BD AF Wang, Chuantong Woodard, Stanley E. Taylor, Bryant D. GP IEEE TI Sensing of Multiple Unrelated Tire Parameters Using Electrically Open Circuit Sensors Having no Electrical Connections SO SAS 2009 - IEEE SENSORS APPLICATIONS SYMPOSIUM, PROCEEDINGS LA English DT Proceedings Paper CT 4th IEEE Sensors Applications Symposium CY FEB 17-19, 2009 CL New Orleans, LA SP IEEE Instrumentat & Measurement Soc DE Electrically open-circuit sensor; tire safety monitoring; magnetic field response sensor; LC resonator; multifunctional tire sensor; SansEC AB All sensors or sensor systems previously used for tire measurements have one common feature - the sensors are part of electrically closed circuits and electrical connections are used to form the closed circuits. In this paper, we present a new tire safety monitoring system using a recently developed method for designing, powering and interrogating sensors developed at NASA. In lieu of sensors being a collection of components assembled using electrical connections, the sensors are patterns of electrically conductive material that can store electric fields and magnetic fields without electrical connections. They are powered using oscillating magnetic fields and respond with their own magnetic fields whose signatures give information about the measured parameters. Because no electrical connections are used to power, communicate with the sensor or to make the sensor, there is no point on the sensor that if damaged, renders the sensor non-functional. Many damage events simply shift the sensor's frequency range. Survivability of the sensor allows it to continue measurement while damaged. The physical quantities to be measured are correlated to the sensor's magnetic field response amplitude, frequency and bandwidth. The proposed method measures wheel speed, rotation angle, direction, acceleration, temperature, damage and wear of tread element by using two or more sensors. In this study, two sensors are used. One of the sensors is coated with temperature sensitive dielectric material. The two sensors working cooperatively are able to measure the seven parameters. The results and multifunctional measurement strategies are presented. C1 [Wang, Chuantong] Natl Inst Aerosp, Hampton, VA 23630 USA. [Woodard, Stanley E.] NASA, Langley Res Ctr, Hampton, VA 23630 USA. [Taylor, Bryant D.] ATK Space Div Res, Hampton, VA 23630 USA. RP Wang, CT (reprint author), Natl Inst Aerosp, Hampton, VA 23630 USA. EM C.Wang@nianet.org; Stanley.E.Woodard@nasa.gov; Bryant.D.Taylor@nasa.gov NR 16 TC 1 Z9 1 U1 0 U2 1 PU IEEE PI NEW YORK PA 345 E 47TH ST, NEW YORK, NY 10017 USA BN 978-1-4244-2786-4 PY 2009 BP 142 EP + PG 2 WC Engineering, Electrical & Electronic; Instruments & Instrumentation; Remote Sensing SC Engineering; Instruments & Instrumentation; Remote Sensing GA BKL67 UT WOS:000268444000030 ER PT B AU Orton, GS Baines, KH Cruikshank, D Cuzzi, JN Krimigis, SM Miller, S Lellouch, E AF Orton, Glenn S. Baines, Kevin H. Cruikshank, Dale Cuzzi, Jeffrey N. Krimigis, Stamatios M. Miller, Steve Lellouch, Emmanuel BE Dougherty, MK Esposito, LW Krimigis, SM TI Review of Knowledge Prior to the Cassini-Huygens Mission and Concurrent Research SO SATURN FROM CASSINI-HUYGENS LA English DT Review; Book Chapter ID HUBBLE-SPACE-TELESCOPE; RESOLVED INFRARED OBSERVATIONS; 1990 EQUATORIAL DISTURBANCE; OUTER SOLAR-SYSTEM; RADIO ASTRONOMY OBSERVATIONS; PARTICLE-SIZE DISTRIBUTIONS; PLANETARY RING-SYSTEMS; SEASONAL CLIMATE MODEL; SATURNS H-3(+) AURORA; AMMONIA ICE PARTICLES AB The scientific achievements of the Cassini-Huygens mission have been based on previous decades of investigations from ground-based observations, an intensive 2-year time span of exploration by three spacecraft (Pioneer Saturn, Voyagers 1 and 2) in 1979-1981, and observations by the Infrared Space Observatory, the International Ultraviolet Explorer, and Hubble Space Telescope. We review both these and research concurrent with the nominal mission which often provided directly supporting results. Saturn's "bulk" composition remains uncertain. Its few discrete cloud features include a hexagon near the sorth pole, and a major episodic storm at the equator. A heterogeneous cloud field at depth was uncovered at 5 mu m. Temperatures are enhanced at Saturn's south pole both from seasonal variations of sunlight and from dynamical forcing. Zonal winds peak near Saturn's equator. Saturn possesses a well-defined ionosphere, but with significant structure and variability. The magnetic field is aligned to within a degree of Saturn's rotation axis. An equatorial ring current of similar to 10(7) A has been inferred, with inner and outer radii of similar to 8 and similar to 16 R-S. Radiation belts at Saturn are well-established up to the edge of the outer rings, and the higherenergy (>1 meV) proton component is readily absorbed by the inner satellites. The magnetosphere includes both a well-developed plasma sheet and a magneto-tail. Radio emissions and plasma waves exist throughout, and the auroral kilometric radiation (SKR), modulated at 10 h 39.4 min, has been widely adopted as a measure of the internal rotation. The plasma population consists principally of protons, but with a heavier component close to the equatorial plane widely assumed to be nitrogen or oxygen. Saturn's ring system is the most accessible in the solar system and consists of three primary components, the A, B and C rings. The A ring contains a large number of spiral density wages generated by gravitational interactions with Saturn's satellites. Other rings include the tenuous D, E, and G rings, and the narrow F ring. Voyager imaging detected "spokes" in the rings and, through occultation studies, an intricate detailed radial structure. Spectroscopic information on the icy satellites reveals the presence of crystalline water ice, mixed with a non-ice surface component with strong UV absorption. Detailed information on the geology of, Saturn's eight largest icy satellites before the Cassini arrival was based entirely on Voyager observations. They were found to be surprisingly heterogeneous, with implied internal activity in Enceladus and the dichotomous albedo of Iapetus being two of the biggest mysteries. Among the smaller satellites are those embedded in Saturn's rings and irregular captured satellites outside the orbits of the co-planar satellites. C1 [Orton, Glenn S.; Baines, Kevin H.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Cruikshank, Dale; Cuzzi, Jeffrey N.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Krimigis, Stamatios M.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA. [Krimigis, Stamatios M.] Acad Athens, Athens 10679, Greece. [Miller, Steve] Univ London Imperial Coll Sci Technol & Med, London WC1E 6BT, England. [Lellouch, Emmanuel] Observ Paris, F-92195 Meudon, France. RP Orton, GS (reprint author), CALTECH, Jet Prop Lab, MS 169-237,4800 Oak Grove Dr, Pasadena, CA 91109 USA. NR 363 TC 4 Z9 4 U1 0 U2 2 PU SPRINGER PI DORDRECHT PA PO BOX 17, 3300 AA DORDRECHT, NETHERLANDS BN 978-1-4020-9216-9 PY 2009 BP 9 EP 54 DI 10.1007/978-1-4020-9217-6_2 D2 10.1007/978-1-4020-9217-6 PG 46 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BMO21 UT WOS:000273026000002 ER PT B AU Johnson, TV Estrada, PR AF Johnson, Torrence V. Estrada, Paul R. BE Dougherty, MK Esposito, LW Krimigis, SM TI Origin of the Saturn System SO SATURN FROM CASSINI-HUYGENS LA English DT Article; Book Chapter ID OUTER SOLAR-SYSTEM; DIFFERENTIATED INTERNAL STRUCTURE; CASSINI IMAGING SCIENCE; LATE HEAVY BOMBARDMENT; GRAVITY-FIELD; GIANT PLANETS; IRREGULAR SATELLITES; INTERIOR STRUCTURE; KUIPER-BELT; COLLISIONAL EVOLUTION AB Cassini mission results are providing new insights into the origin of the Saturn system and giant planet satellite systems generally. The chapter discusses current models for the formation of giant planets and their satellites and reviews major Cassini findings which help advance our understanding of the system's formation and evolution to its current state. C1 [Johnson, Torrence V.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Estrada, Paul R.] SETI Inst, Carl Sagan Ctr, Mountain View, CA 94043 USA. RP Johnson, TV (reprint author), CALTECH, Jet Prop Lab, MS 301-345E,4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM Torrence.V.Johnson@jpl.nasa.gov; Paul.R.Estrada@nasa.gov NR 148 TC 7 Z9 7 U1 0 U2 0 PU SPRINGER PI DORDRECHT PA PO BOX 17, 3300 AA DORDRECHT, NETHERLANDS BN 978-1-4020-9216-9 PY 2009 BP 55 EP 74 DI 10.1007/978-1-4020-9217-6_3 D2 10.1007/978-1-4020-9217-6 PG 20 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BMO21 UT WOS:000273026000003 ER PT B AU Hubbard, WB Dougherty, MK Gautier, D Jacobson, R AF Hubbard, William B. Dougherty, Michele K. Gautier, Daniel Jacobson, Robert BE Dougherty, MK Esposito, LW Krimigis, SM TI The Interior of Saturn SO SATURN FROM CASSINI-HUYGENS LA English DT Article; Book Chapter DE Saturn interior; Saturn atmosphere; Saturn rotation; Jupiter interior ID INTERNAL STRUCTURE; GIANT PLANETS; HELIUM; HYDROGEN; OCCULTATION; ATMOSPHERE; ABUNDANCE; PRESSURE; EQUATION; JUPITER AB A source of uncertainty in Saturn interior models is the lack of a unique rotation rate to be ascribed to the deep (metallic-hydrogen) interior. As a result, models are not uniquely constrained by measured gravitational multiple coefficients. Further uncertainty is associated with the effect of a multiplicity of rotation periods due to zonal flows of unknown magnitude and depth (and therefore unknown mass). Nevertheless, the inference that Saturn has a large core of mass 15-20 ME (Earth masses) is robust. The equation of state of dense hydrogen-helium mixtures is one area where uncertainty has been much reduced, thanks to new first-principles simulations. However, because there is still uncertainty in Saturn's interior temperature profile, a variety of mantle metallicities and core masses could still fit the constraints, and the question of interior helium separation is still unsettled. C1 [Hubbard, William B.] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA. [Dougherty, Michele K.] Univ London Imperial Coll Sci Technol & Med, Dept Phys, London, England. [Jacobson, Robert] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. [Gautier, Daniel] Observ Paris Site Meudon, Paris, France. RP Hubbard, WB (reprint author), Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA. NR 22 TC 9 Z9 9 U1 0 U2 0 PU SPRINGER PI DORDRECHT PA PO BOX 17, 3300 AA DORDRECHT, NETHERLANDS BN 978-1-4020-9216-9 PY 2009 BP 75 EP 81 DI 10.1007/978-1-4020-9217-6_4 D2 10.1007/978-1-4020-9217-6 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BMO21 UT WOS:000273026000004 ER PT B AU Del Genio, AD Achterberg, RK Baines, KH Flasar, FM Read, PL Sanchez-Lavega, A Showman, AP AF Del Genio, Anthony D. Achterberg, Richard K. Baines, Kevin H. Flasar, F. Michael Read, Peter L. Sanchez-Lavega, Agustin Showman, Adam P. BE Dougherty, MK Esposito, LW Krimigis, SM TI Saturn Atmospheric Structure and Dynamics SO SATURN FROM CASSINI-HUYGENS LA English DT Article; Book Chapter ID SHALLOW-WATER TURBULENCE; HUBBLE-SPACE-TELESCOPE; NORTH POLAR SPOT; GREAT RED SPOT; VOYAGER INFRARED MEASUREMENTS; POTENTIAL-VORTICITY DYNAMICS; 1990 EQUATORIAL DISTURBANCE; ROTATING SPHERICAL-SHELLS; JUPITER UPPER TROPOSPHERE; LARGE-SCALE INSTABILITIES AB Saturn inhabits a dynamical regime of rapidly rotating, internally heated atmospheres similar to Jupiter. Zonal winds have remained fairly steady since the time of Voyager except in the equatorial zone and slightly stronger winds occur at deeper levels. Eddies supply energy to the jets at a rate somewhat less than on Jupiter and mix potential vorticity near westward jets. Convective clouds exist preferentially in cyclonic shear regions as on Jupiter but also near jets, including major outbreaks near 35 S associated with Saturn electrostatic discharges, and in sporadic giant equatorial storms perhaps generated froth frequent events at depth. The implied meridional circulation at and below the visible cloud tops consists of upwelling (downwelling) at cyclonic (anti-cyclonic) shear latitudes. Thermal winds decay upward above the clouds, implying a reversal of the circulation there. Warm-core vortices with associated cyclonic circulations exist at both poles, including surrounding thick high clouds at the south pole. Disequilibrium gas concentrations in the tropical upper troposphere imply rising motion there. The radiative-convective boundary and tropopause occur at higher pressure in the southern (summer) hemisphere due to greater penetration of solar heating there. A temperature "knee" of warm air below the tropopause, perhaps due to haze heating, is stronger in the summer hemisphere as well. Saturn's south polar stratosphere is warmer than predicted by radiative models and enhanced in ethane, suggesting subsidence-driven adiabatic warming there. Recent modeling advances suggest that shallow weather layer theories of jet pumping may be viable if water condensation is the source of energy input driving the flow, and that deep convective cylinder models with a sufficiently large tangent cylinder radius can reproduce observed flow features as well. C1 [Del Genio, Anthony D.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA. [Achterberg, Richard K.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Baines, Kevin H.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Flasar, F. Michael] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Sanchez-Lavega, Agustin] Univ Basque Country, Dept Fis Aplicada, Bilbao 48013, Spain. [Showman, Adam P.] Univ Arizona, Dept Planetary Sci, Tucson, AZ 85721 USA. [Showman, Adam P.] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA. [Read, Peter L.] Clarendon Lab, Oxford OX1 3PU, England. RP Del Genio, AD (reprint author), NASA, Goddard Inst Space Studies, 2880 Broadway, New York, NY 10025 USA. RI Flasar, F Michael/C-8509-2012; OI Sanchez-Lavega, Agustin/0000-0001-7355-1522 NR 225 TC 26 Z9 26 U1 1 U2 6 PU SPRINGER PI DORDRECHT PA PO BOX 17, 3300 AA DORDRECHT, NETHERLANDS BN 978-1-4020-9216-9 PY 2009 BP 113 EP 159 DI 10.1007/978-1-4020-9217-6_6 D2 10.1007/978-1-4020-9217-6 PG 47 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BMO21 UT WOS:000273026000006 ER PT B AU West, RA Baines, KH Karkoschka, E Sanchez-Lavega, A AF West, R. A. Baines, K. H. Karkoschka, E. Sanchez-Lavega, A. BE Dougherty, MK Esposito, LW Krimigis, SM TI Clouds and Aerosols in Saturn's Atmosphere SO SATURN FROM CASSINI-HUYGENS LA English DT Article; Book Chapter ID 1990 EQUATORIAL DISTURBANCE; SPACE TELESCOPE OBSERVATIONS; NEAR-IR SPECTROPHOTOMETRY; AMMONIA ICE; JOVIAN PLANETS; VERTICAL STRUCTURE; UPPER TROPOSPHERE; HAZE FORMATION; JUPITER; PHOTOMETRY AB In this chapter we review the photochemical and thermochemical equilibrium theories for the formation of condensate clouds and photochemical haze in Saturn's upper troposphere and stratosphere and show the relevant observations from ground-based and spacecraft instruments. Based on thermochemical equilibrium models we expect ammonia ice crystals to dominate in the high troposphere. There is very little spectral evidence to confirm this idea. Thanks to a stellar occultation observed by the Cassini VIMS instrument we now have spectral evidence for a hydrocarbon stratospheric haze component, and we still seek evidence for an expected diphosphine stratospheric haze component. The vertical distributions of stratospheric and upper tropospheric hazes have been mapped well with ground-based and Hubble Space telescope data, and Cassini data are beginning to add to this picture. Polar stratospheric aerosols are dark at UV wavelengths and exhibit strong Rayleigh-like polarization which suggests that auroral processes are important for their formation as is the case for the jovian polar stratospheric haze. The cloud and haze structure exhibits a variety of temporal variation, including seasonal change, long-term secular change near the equator, and short-term changes with a complicated latitudinal structure, and still not understood. Cassini instruments, especially the VIMS instrument, show an abundance of small-scale structure (convective clouds) at a pressure near 2 bar. C1 [West, R. A.; Baines, K. H.] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. [Karkoschka, E.] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA. [Sanchez-Lavega, A.] Univ Basque Country, ETS Ingenieros, Dept Fis Aplicada 1, E-48080 Bilbao, Spain. RP West, RA (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91125 USA. OI Sanchez-Lavega, Agustin/0000-0001-7355-1522 NR 59 TC 26 Z9 26 U1 0 U2 1 PU SPRINGER PI DORDRECHT PA PO BOX 17, 3300 AA DORDRECHT, NETHERLANDS BN 978-1-4020-9216-9 PY 2009 BP 161 EP 179 DI 10.1007/978-1-4020-9217-6_7 D2 10.1007/978-1-4020-9217-6 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BMO21 UT WOS:000273026000007 ER PT B AU Nagy, AF Kliore, AJ Mendillo, M Miller, S Moore, L Moses, JI Muller-Wodarg, I Shemansky, D AF Nagy, Andrew F. Kliore, Arvydas J. Mendillo, Michael Miller, Steve Moore, Luke Moses, Julianne I. Mueller-Wodarg, Ingo Shemansky, Don BE Dougherty, MK Esposito, LW Krimigis, SM TI Upper Atmosphere and Ionosphere of Saturn SO SATURN FROM CASSINI-HUYGENS LA English DT Article; Book Chapter ID EXTREME-ULTRAVIOLET OBSERVATIONS; JOVIAN UPPER-ATMOSPHERE; PLANETARY-ATMOSPHERES; OCCULTATION MEASUREMENTS; THERMAL PROFILES; CROSS-SECTIONS; OUTER PLANETS; JUPITER; H-3(+); THERMOSPHERE AB This chapter summarizes our current understanding of the upper atmosphere and ionosphere of Saturn. We summarize the available observations and the various relevant models associated with these regions. We describe what is currently known, outline any controversies and indicate how future observations can help in advancing our understanding of the various controlling physical and chemical processes. C1 [Nagy, Andrew F.] Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA. [Kliore, Arvydas J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Mendillo, Michael; Moore, Luke] Boston Univ, Ctr Space Phys, Boston, MA 02215 USA. [Miller, Steve] UCL, Dept Phys & Astron, London WC1E 6BT, England. [Moses, Julianne I.] Lunar & Planetary Inst, Houston, TX 77058 USA. [Mueller-Wodarg, Ingo] Univ London Imperial Coll Sci Technol & Med, London SW7 2AZ, England. [Shemansky, Don] Planetary & Space Sci Div, Pasadena, CA 91107 USA. RP Nagy, AF (reprint author), Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA. RI Mendillo, Michael /H-4397-2014; Moses, Julianne/I-2151-2013 OI Moses, Julianne/0000-0002-8837-0035 NR 106 TC 28 Z9 28 U1 0 U2 5 PU SPRINGER PI DORDRECHT PA PO BOX 17, 3300 AA DORDRECHT, NETHERLANDS BN 978-1-4020-9216-9 PY 2009 BP 181 EP 201 DI 10.1007/978-1-4020-9217-6_8 D2 10.1007/978-1-4020-9217-6 PG 21 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BMO21 UT WOS:000273026000008 ER PT B AU Mauk, BH Hamilton, DC Hill, TW Hospodarsky, GB Johnson, RE Paranicas, C Roussos, E Russell, CT Shemansky, DE Sittler, EC Thorne, RM AF Mauk, B. H. Hamilton, D. C. Hill, T. W. Hospodarsky, G. B. Johnson, R. E. Paranicas, C. Roussos, E. Russell, C. T. Shemansky, D. E. Sittler, E. C., Jr. Thorne, R. M. BE Dougherty, MK Esposito, LW Krimigis, SM TI Fundamental Plasma Processes in Saturn's Magnetosphere SO SATURN FROM CASSINI-HUYGENS LA English DT Article; Book Chapter ID NARROWBAND ELECTROMAGNETIC EMISSIONS; NONTHERMAL CONTINUUM RADIATION; INTERPLANETARY MAGNETIC-FIELD; RADIO ASTRONOMY OBSERVATIONS; ENERGETIC CHARGED-PARTICLES; PITCH-ANGLE DIFFUSION; NEUTRAL CLOUD THEORY; ION-CYCLOTRON WAVES; DEPLETED FLUX TUBES; JOVIAN MAGNETOSPHERE AB In this chapter, we review selected fundamental plasma processes that control the extensive space environment, or magnetosphere, of Saturn (see Chapter 9, for the global context). This writing occurs at a point in time when some measure of maturity has been achieved in our understanding of the operations of Saturn's magnetosphere and its relationship to those of Earth and Jupiter. Our understanding of planetary magnetospheres has exploded in the past decade or so partly because of the presence of orbiting spacecraft (Galileo and Cassini) as well as remote sensing assets (e.g., Hubble Space Telescope). This book and chapter are intended to take stock of where we are in our understanding of Saturn's magnetosphere following the successful return and analysis of extensive sets of Cassini data. The end of the prime mission provides us with an opportunity to consolidate older and newer work to provide guidance for continuing investigations. C1 [Mauk, B. H.; Paranicas, C.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD USA. [Hamilton, D. C.] Univ Maryland, Dept Phys, College Pk, MD 20742 USA. [Hill, T. W.] Rice Univ, Dept Phys & Astron, Houston, TX USA. [Hospodarsky, G. B.] Univ Iowa, Dept Phys & Astron, Iowa City, IA 52242 USA. [Johnson, R. E.] Univ Virginia, Dept Mat Sci & Engn, Charlottesville, VA USA. [Russell, C. T.] Univ Calif Los Angeles, Inst Geophys & Planetary Phys, Los Angeles, CA 90024 USA. [Shemansky, D. E.] Planetary & Space Sci Div, Pasadena, CA USA. [Sittler, E. C., Jr.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Thorne, R. M.] Univ Calif Los Angeles, Dept Atmospher & Ocean Sci, Los Angeles, CA 90024 USA. [Roussos, E.] Max Planck Inst Sonnensyst Forsch, D-37191 Katlenburg Lindau, Germany. RP Mauk, BH (reprint author), Johns Hopkins Univ, Appl Phys Lab, Laurel, MD USA. EM Barry.mauk@jhuapl.edu RI Paranicas, Christopher/B-1470-2016; Mauk, Barry/E-8420-2017; OI Paranicas, Christopher/0000-0002-4391-8255; Mauk, Barry/0000-0001-9789-3797; Hamilton, Douglas/0000-0001-6103-8019; Hospodarsky, George/0000-0001-9200-9878; Roussos, Elias/0000-0002-5699-0678; Russell, Christopher/0000-0003-1639-8298 NR 310 TC 47 Z9 47 U1 0 U2 2 PU SPRINGER PI DORDRECHT PA PO BOX 17, 3300 AA DORDRECHT, NETHERLANDS BN 978-1-4020-9216-9 PY 2009 BP 281 EP 331 DI 10.1007/978-1-4020-9217-6_11 D2 10.1007/978-1-4020-9217-6 PG 51 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BMO21 UT WOS:000273026000011 ER PT B AU Schmidt, J Ohtsuki, K Rappaport, N Salo, H Spahn, F AF Schmidt, Juergen Ohtsuki, Keiji Rappaport, Nicole Salo, Heikki Spahn, Frank BE Dougherty, MK Esposito, LW Krimigis, SM TI Dynamics of Saturn's Dense Rings SO SATURN FROM CASSINI-HUYGENS LA English DT Article; Book Chapter ID PARTICLE-SIZE DISTRIBUTIONS; AZIMUTHAL BRIGHTNESS VARIATIONS; VOYAGER-1 RADIO OCCULTATION; SELF-GRAVITATING PARTICLES; NARROW PLANETARY RINGS; OPTICAL DEPTH PROFILE; N-BODY SIMULATIONS; NEARBY GAP EDGE; F-RING; B-RING AB The Cassini mission to Saturn opened a new era in the research of planetary rings, bringing data in unprecedented detail, monitoring the structure and properties of Saturn's ring system. The question of ring dynamics is to identify and understand underlying physical processes and to connect them to the observations in terms of mathematical models and computer simulations. For Saturn's dense rings important physical processes are dissipative collisions between ring particles, their motion in Saturn's gravity field, their mutual self-gravity, and the gravitational interaction with Saturn's moons, exterior to or embedded in the rings. The importance of the rings' self-gravity became strikingly clear from the identification of gravitational wakes in Cassini data nearly everywhere in the A and B rings. Self-gravity wakes imply that the rings are in a flat, dynamically cold state, ring particles colliding very dissipatively, being densely packed in the ring plane, continuously forming transient gravitationally bound opaque clumps, that are disrupted again by shear on orbital timescales. Current mathematical dynamical models usually treat self-gravity in an approximate manner, which does not lead to a wake state. The dense packing of ring particles, in turn, strongly influences the collisional dynamics, since the mean free path of the particles is then comparable to or smaller than the particle size. This leads to a strong nonlocal component of pressure and momentum transport, which determines the viscous evolution of the rings, the damping of density waves, as well as the stability properties of the ring's flow. A strong nonlocal contribution to viscosity is, for instance, favorable for viscous overstability, leading to axisymmetric waves of about 100 m wavelength. Such wavelike perturbations in the ring's opacity, consistent with overstability, are seen in Cassini stellar and radio occultations. A classical topic of ring dynamics is the interaction of moons and rings. On the one hand, there are exterior moons with resonances in the rings, creating numerous density and bending waves. With the large sets of Cassini occultation and imaging data, improved estimates of the ring surface mass density and viscosity are obtained from fits of the observations to dynamical models. On the other hand, the embedded moons Pan and Daphnis open the Encke and Keeler gaps, respectively, and moonlets in the rings, too small to open a circumferential gap, are found to produce a characteristic propeller structure. Comparison between theoretical studies and Cassini observations of thermal emission from the rings provides constraints on spin rates of ring particles, which are otherwise not directly observable. The size distribution of particles and small moonlets embedded in the rings, together with the observed shapes and internal densities of small moons just exterior to the rings, underline the importance of accretion and fragmentation for the dynamical evolution of Saturn's ring system. C1 [Schmidt, Juergen; Spahn, Frank] Univ Potsdam, Inst F Phys & Astron, Potsdam, Germany. [Rappaport, Nicole] JPL, Pasadena, CA USA. [Salo, Heikki] Univ Oulu, Div Astron, Dept Phys Sci, Oulu, Finland. [Ohtsuki, Keiji] Univ Colorado, Atmospher & Space Phys Lab, Boulder, CO 80309 USA. [Ohtsuki, Keiji] Kobe Univ, Dept Earth & Planet Sci, Kobe, Hyogo, Japan. [Ohtsuki, Keiji] Kobe Univ, Ctr Planet Sci, Kobe, Hyogo, Japan. RP Schmidt, J (reprint author), Univ Potsdam, Inst F Phys & Astron, Potsdam, Germany. NR 278 TC 34 Z9 34 U1 0 U2 3 PU SPRINGER PI DORDRECHT PA PO BOX 17, 3300 AA DORDRECHT, NETHERLANDS BN 978-1-4020-9216-9 PY 2009 BP 413 EP 458 DI 10.1007/978-1-4020-9217-6_14 D2 10.1007/978-1-4020-9217-6 PG 46 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BMO21 UT WOS:000273026000014 ER PT B AU Cuzzi, J Clark, R Filacchione, G French, R Johnson, R Marouf, E Spilker, L AF Cuzzi, Jeff Clark, Roger Filacchione, Gianrico French, Richard Johnson, Robert Marouf, Essam Spilker, Linda BE Dougherty, MK Esposito, LW Krimigis, SM TI Ring Particle Composition and Size Distribution SO SATURN FROM CASSINI-HUYGENS LA English DT Article; Book Chapter ID BIDIRECTIONAL REFLECTANCE SPECTROSCOPY; SATURNS MAIN RINGS; POLYCYCLIC AROMATIC-HYDROCARBONS; VOYAGER-1 RADIO OCCULTATION; INFRARED OPTICAL-PROPERTIES; SOLAR-SYSTEM BODIES; WATER-VAPOR PLUME; CASSINI-VIMS; PLANETARY RINGS; PHASE CURVES AB We review recent progress concerning the composition and size distribution of the particles in Saturn's main ring system, and describe how these properties vary from place to place. We discuss how the particle size distribution is measured, and how it varies radially. We note the discovery of unusually large "particles" in restricted radial bands. We discuss the properties of the grainy regoliths of the ring particles. We review advances in understanding of ring particle composition from spectrophotometry at UV, visual and near-IR wavelengths, multicolor photometry at visual wavelengths, and thermal emission. We discuss the observed ring atmosphere and its interpretation and, briefly, models of the evolution of ring composition. We connect the ring composition with what has been learned recently about the composition of other icy objects in the Saturn system and beyond. Because the rings are so thoroughly and rapidly structurally evolved, the composition of the rings may be our best clue as to their origin; however, the evolution of ring particle composition over time must first be understood. C1 [Cuzzi, Jeff] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Clark, Roger] US Geol Survey, Denver, CO 80225 USA. [French, Richard] Wellesley Coll, Wellesley, MA 02181 USA. [Johnson, Robert] Univ Virginia, Charlottesville, VA USA. [Marouf, Essam] San Jose State Univ, San Jose, CA 95192 USA. [Spilker, Linda] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Filacchione, Gianrico] Ist Astrofis Spaziale & Fis Cosm, Rome, Italy. RP Cuzzi, J (reprint author), NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. OI Filacchione, Gianrico/0000-0001-9567-0055 NR 197 TC 57 Z9 57 U1 0 U2 8 PU SPRINGER PI DORDRECHT PA PO BOX 17, 3300 AA DORDRECHT, NETHERLANDS BN 978-1-4020-9216-9 PY 2009 BP 459 EP 509 DI 10.1007/978-1-4020-9217-6_15 D2 10.1007/978-1-4020-9217-6 PG 51 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BMO21 UT WOS:000273026000015 ER PT B AU Matson, DL Castillo-Rogez, JC Schubert, G Sotin, C McKinnon, WB AF Matson, Dennis L. Castillo-Rogez, Julie C. Schubert, Gerald Sotin, Christophe McKinnon, William B. BE Dougherty, MK Esposito, LW Krimigis, SM TI The Thermal Evolution and Internal Structure of Saturn's Mid-Sized Icy Satellites SO SATURN FROM CASSINI-HUYGENS LA English DT Article; Book Chapter ID TEMPERATURE-DEPENDENT VISCOSITY; INFINITE PRANDTL NUMBER; STAGNANT LID CONVECTION; CHONDRITE PARENT BODIES; LATE HEAVY BOMBARDMENT; OUTER SOLAR-SYSTEM; INTERIOR STRUCTURE; LIQUID WATER; GALILEAN SATELLITES; TERRESTRIAL PLANETS AB The Cassini-Huygens mission is returning new geophysical data for the midsize, icy satellites of Saturn (i.e., satellites with radii between 100 and 1,000 km). These data have enabled a new generation of geophysical model studies for Phoebe, Iapetus, Rhea, Mimas, Tethys, Dione, as well as Enceladus (which is addressed in a separate chapter in this book). In the present chapter we consider the new model studies that have reported significant results elucidating the evolutionary histories and internal structures of these satellites. Those results have included their age, the development of their internal structures and mineralogies, which for greatest fidelity must be done concomitantly with coupled dynamical evolutions. Surface areas, volumes, bulk densities, spin rates, orbit inclinations, eccentricities, and distance from Saturn have changed as the satellites have aged. Heat is required to power the satellites' evolution, but is not overly abundant for the midsized satellites. All sources of heat must be evaluated and taken into account. This includes their intensities and when they occur and are available to facilitate evolution, both internal and dynamical. The mechanisms of heat transport must also be included. However, to model these to high fidelity the material properties of the satellite interiors must be accurately known. This is not the case. Thus, much of the chapter is devoted to discussion of what is known about these properties and how the uncertainties affect the estimation of heat sources, transport processes, and the consequential changes in composition and evolution. Phoebe has an oblate shape that may be in equilibrium with its spin period of similar to 9.3 h. Its orbital properties suggest that it is not one of the regular satellites, but is a captured body. Its density is higher than that of the other satellites, consistent with formation in the solar nebula rather than from material around Saturn. Oblate shape and high density are unusual for objects in this size range, and may indicate that Phoebe was heated by Al-26 decay soon after its formation, which is consistent with some models of the origin of Kuiper-Belt objects. lapetus has the shape of a hydrostatic body with a rotation period of 16 h. It subsequently despun to its current synchronous rotation state, similar to 79 day period. These observations are sufficient to constrain the required heating in Iapetus' early history, suggesting that it formed several My after CAI condensation. Since Saturn had to be present for Iapetus to form, this date also constrains the age of Saturn and how long it took to form. Both shape and gravitational data are available for Rhea. Gravity data were obtained from the single Cassini flyby during the prime mission and within the uncertainties cannot distinguish between hydrostatic and non-hydrostatic gravitational fields. Both Dione and Tethys display evidence of smooth terrains, with Dione's appearing considerably younger. Both are conceivably linked to tidal heating in the past, but the low rock abundance within Tethys and the lack of eccentricity excitation of Tethys' orbit today make explaining this satellite's geology challenging. C1 [Matson, Dennis L.; Castillo-Rogez, Julie C.; Sotin, Christophe] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Schubert, Gerald] Univ Calif Los Angeles, Los Angeles, CA 90095 USA. [McKinnon, William B.] Washington Univ, St Louis, MO 63139 USA. RP Matson, DL (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. NR 178 TC 17 Z9 17 U1 2 U2 3 PU SPRINGER PI DORDRECHT PA PO BOX 17, 3300 AA DORDRECHT, NETHERLANDS BN 978-1-4020-9216-9 PY 2009 BP 577 EP 612 DI 10.1007/978-1-4020-9217-6_18 D2 10.1007/978-1-4020-9217-6 PG 36 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BMO21 UT WOS:000273026000018 ER PT B AU Dones, L Chapman, CR McKinnon, WB Melosh, HJ Kirchoff, MR Neukum, G Zahnle, KJ AF Dones, Luke Chapman, Clark R. McKinnon, William B. Melosh, H. Jay Kirchoff, Michelle R. Neukum, Gerhard Zahnle, Kevin J. BE Dougherty, MK Esposito, LW Krimigis, SM TI Icy Satellites of Saturn: Impact Cratering and Age Determination SO SATURN FROM CASSINI-HUYGENS LA English DT Article; Book Chapter ID LATE HEAVY BOMBARDMENT; JUPITER-FAMILY COMETS; TERRESTRIAL PLANET FORMATION; JOVIAN TROJAN ASTEROIDS; TRANS-NEPTUNIAN BODIES; KUIPER-BELT OBJECTS; SHORT-PERIOD COMETS; OUTER SOLAR-SYSTEM; SHOEMAKER-LEVY 9; IRREGULAR SATELLITES AB Saturn is the first giant planet to be visited by an orbiting spacecraft that can transmit large amounts of data to Earth. Crater counts on satellites from Phoebe inward to the regular satellites and ring moons are providing unprecedented insights into the origin and time histories of the impacting populations. Many Voyager-era scientists concluded that the satellites had been struck by at least two populations of impactors. In this view, the Population I impactors, which were generally judged to be "comets" orbiting the Sun, formed most of the larger and older craters, while Population II impactors, interpreted as Saturn-orbiting ejecta from impacts on satellites, produced most of the smaller and younger craters. Voyager data also implied that all of the "ring moons;" and probably some of the mid-sized classical moons, had been catastrophically disrupted and reaccreted since they formed. We examine models of the primary impactor populations in the Saturn system. At the present time, "ecliptic comets," which likely originate in the Kuiper Belt/Scattered Disk, are predicted to dominate impacts on the regular satellites and ring moons, but the models require extrapolations in size (from the observed Kuiper Belt Objects to the much smaller bodies that produce the craters) or in distance (from the known active Jupiter family comets to 9.5 AU). Phoebe, Iapetus, and perhaps even moons closer to Saturn have been struck by irregular satellites as well. We describe the Nice model, which provides a plausible mechanism by which the entire Solar System might have experienced an era of heavy bombardment long after the planets formed. We then discuss the three cratering chronologies, including one based upon the Nice model, that have been used to infer surface ages from crater densities on the saturnian satellites. After reviewing scaling relations between the properties of impactors and the craters they produce, we provide model estimates of the present-day rate at which comets impact, and catastrophically disrupt, the saturnian moons. Finally, we present crater counts on the satellites from two different groups. Many of the heavily cratered terrains appear to be nearly saturated, so it is difficult to infer the provenance of the impactors from crater counts alone. More large craters have been found on Iapetus than on any other satellite. Enceladus displays an enormous range of surface ages, ranging from the old mid-latitude plains to the extremely young South Polar Terrain. Cassini images provide some evidence for the reality of "Population II". Most of the observed craters may have formed in one or more "cataclysms," but more work is needed to determine the roles of heliocentric and planetocentric bodies in creating the craters. C1 [Dones, Luke; Chapman, Clark R.] SW Res Inst, Boulder, CO 80302 USA. [McKinnon, William B.] Washington Univ, St Louis, MO 63130 USA. [Melosh, H. Jay] Univ Arizona, Tucson, AZ 85721 USA. [Kirchoff, Michelle R.] Lunar & Planetary Inst, Houston, TX 77058 USA. [Neukum, Gerhard] Free Univ Berlin, D-12249 Berlin, Germany. [Zahnle, Kevin J.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Dones, L (reprint author), SW Res Inst, Boulder, CO 80302 USA. NR 194 TC 30 Z9 30 U1 1 U2 2 PU SPRINGER PI DORDRECHT PA PO BOX 17, 3300 AA DORDRECHT, NETHERLANDS BN 978-1-4020-9216-9 PY 2009 BP 613 EP 635 DI 10.1007/978-1-4020-9217-6_19 D2 10.1007/978-1-4020-9217-6 PG 23 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BMO21 UT WOS:000273026000019 ER PT B AU Jaumann, R Clark, RN Nimmo, F Hendrix, AR Buratti, BJ Denk, T Moore, JM Schenk, PM Ostro, SJ Srama, R AF Jaumann, Ralf Clark, Roger N. Nimmo, Francis Hendrix, Amanda R. Buratti, Bonnie J. Denk, Tilmann Moore, Jeffrey M. Schenk, Paul M. Ostro, Steve J. Srama, Ralf BE Dougherty, MK Esposito, LW Krimigis, SM TI Icy Satellites: Geological Evolution and Surface Processes SO SATURN FROM CASSINI-HUYGENS LA English DT Article; Book Chapter ID INFRARED MAPPING SPECTROMETER; CASSINI IMAGING SCIENCE; BIDIRECTIONAL REFLECTANCE SPECTROSCOPY; GALILEO ULTRAVIOLET SPECTROMETER; SATURNS SMALL SATELLITES; TITAN RADAR MAPPER; E-RING; WATER VOLCANISM; DARK MATERIAL; POLAR WANDER AB The sizes of the Saturnian icy satellites range from similar to 1,500 km in diameter (Rhea) to similar to 20 km (Calypso), and even smaller 'rocks' of only a kilometer in diameter are common in the system. All these bodies exhibit remarkable, unique features and unexpected diversity. In this chapter, we will mostly focus on the 'medium-sized icy objects' Mimas, Tethys, Dione, Rhea, Iapetus, Phoebe and Hyperion, and consider small objects only where appropriate, whereas Titan and Enceladus will be described in separate chapters. Mimas and Tethys show impact craters caused by bodies that were almost large enough to break them apart. Iapetus is unique in the Saturnian system because of its extreme global brightness dichotomy. Tectonic activity varies widely - from inactive Mimas through extensional terrains on Rhea and Dione to the current cryovolcanic eruptions on Enceladus - and is not necessarily correlated with predicted tidal stresses. Likely sources of stress include impacts, despinning, reorientation and volume changes. Accretion of dark material originating from outside the Saturnian system may explain the surface contamination that prevails in the whole satellite system, while coating by Saturn's E-ring particles brightens the inner satellites. So far, among the surprising Cassini discoveries are the volcanic activity on Enceladus, the sponge-like appearance of Hyperion and the equatorial ridge on Iapetus - unique features in the solar system. The bright-ray system on Rhea was caused by a relatively recent medium impact which formed a similar to 40 km crater at 12 degrees S latitude, 112 degrees W longitude, while the wispy streaks on Dione and Rhea are of tectonic origin. Compositional mapping shows that the dark material on Iapetus is composed of organics, CO2 mixed with H2O ice, and metallic iron, and also exhibits possible signatures of ammonia, bound water, H-2 or OH-bearing minerals, and a number of as-yet unidentified substances. The spatial pattern, Rayleigh scattering effect, and spectral properties argue that the dark material on Iapetus is only a thin coating on its surface. Radar data indicate that the thickness of the dark layers can be no more than a few decimeters; this is also consistent with the discovery of small bright-ray and bright-floor craters within the dark terrain. Moreover, several spectral features of the dark material match those seen on Phoebe, Iapetus, Hyperion, Dione and Epimetheus as well as in the F-ring and the Cassini Division, implying that throughout the Saturnian system. All dark material appears to have a high content of metallic iron and a small content of nano-phase hematite. However, the complete composition of the dark material is still unresolved, and additional laboratory work is required. As previously concluded for Phoebe, the dark material appears to have originated external to the Saturnian system. The icy satellites of Saturn offer an unrivalled natural laboratory for understanding the geological diversity of different-sized icy satellites and their interactions within a complex planetary system. C1 [Jaumann, Ralf] Inst Planetary Res, DLR, D-12489 Berlin, Germany. [Jaumann, Ralf; Denk, Tilmann] Free Univ Berlin, Inst Geol Sci, D-12249 Berlin, Germany. [Clark, Roger N.] US Geol Survey, Denver Fed Ctr, Denver, CO 80225 USA. [Nimmo, Francis] Univ Calif Santa Cruz, Dept Earth & Planetary Sci, Santa Cruz, CA 95064 USA. [Hendrix, Amanda R.; Buratti, Bonnie J.; Ostro, Steve J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Moore, Jeffrey M.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Schenk, Paul M.] Lunar & Planetary Inst, Houston, TX 77058 USA. [Srama, Ralf] Max Planck Inst Kernphys, D-69117 Heidelberg, Germany. RP Jaumann, R (reprint author), Inst Planetary Res, DLR, Rutherfordstr 2, D-12489 Berlin, Germany. NR 300 TC 28 Z9 28 U1 0 U2 3 PU SPRINGER PI DORDRECHT PA PO BOX 17, 3300 AA DORDRECHT, NETHERLANDS BN 978-1-4020-9216-9 PY 2009 BP 637 EP 681 DI 10.1007/978-1-4020-9217-6_20 D2 10.1007/978-1-4020-9217-6 PG 45 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BMO21 UT WOS:000273026000020 ER PT B AU Spencer, JR Barr, AC Esposito, LW Helfenstein, P Ingersoll, AP Jaumann, R McKay, CP Nimmo, F Waite, JH AF Spencer, John R. Barr, Amy C. Esposito, Larry W. Helfenstein, Paul Ingersoll, Andrew P. Jaumann, Ralf McKay, Christopher P. Nimmo, Francis Waite, J. Hunter BE Dougherty, MK Esposito, LW Krimigis, SM TI Enceladus: An Active Cryovolcanic Satellite SO SATURN FROM CASSINI-HUYGENS LA English DT Article; Book Chapter ID SATURNS E-RING; OUTER SOLAR-SYSTEM; NEAR-INFRARED SPECTRA; SOUTH-POLAR FRACTURES; TIDAL DISSIPATION; ICY SATELLITES; HYDROTHERMAL SYSTEMS; VISCOELASTIC MODELS; INTERNAL STRUCTURE; DUST MEASUREMENTS AB Enceladus is one of the most remarkable satellites in the solar system, as revealed by Cassini's detection of active plumes erupting from warm fractures near its south pole. This discovery makes Enceladus the only icy satellite known to exhibit ongoing internally driven geological activity. The activity is presumably powered by tidal heating maintained by Enceladus' 2:1 mean-motion resonance with Dione, but many questions remain. For instance, it appears difficult or impossible to maintain the currently observed radiated power (probably at least 6 GW) in steady state. It is also not clear how Enceladus first entered its current self-maintaining warm and dissipative state-initial heating from non-tidal sources is probably required. There are also many unanswered questions about Enceladus' interior. The silicate fraction inferred from its density of 1.68 g cm(-2) is probably differentiated into a core, though we have not direct evidence for differentiation. Above the core there is probably a global or regional liquid water layer, inferred from several models of tidal heating, and an ice shell thick enough to support the similar to 1 km amplitude topography seen on Enceladus. It is possible that dissipation is largely localized beneath the south polar region. Enceladus' surface geology, ranging from moderately cratered terrain to the virtually crater-free active south polar region, is highly diverse, tectonically complex, and remarkably symmetrical about the rotation axis and the direction to Saturn. South polar activity is concentrated along the four "tiger stripe" fractures, which radiate heat at temperatures up to at least 167 K and are the source of multiple plumes ejecting similar to 200 kg s(-1) of H2O vapor along with significant N-2 (or C2H4), CO2, CH4, NH3, and higher-mass hydrocarbons. The escaping gas maintains Saturn's neutral gas torus, and the plumes also eject a large number of micron-sized H2O ice grains that populate Saturn's E-ring. The mechanism that powers the plumes is not well understood, and whether liquid water is involved is a subject of active debate. Enceladus provides perhaps the most promising potential habitat for life in the outer solar system, and the active plumes allow the unique opportunity for direct sampling of that zone. Enceladus is thus a prime target for Cassini's continued exploration of the Saturn system, and will be a tempting target for future missions. C1 [Spencer, John R.; Barr, Amy C.] SW Res Inst, Boulder, CO USA. [Waite, J. Hunter] SW Res Inst, San Antonio, TX USA. [Esposito, Larry W.] Univ Colorado, LASP, Boulder, CO 80309 USA. [Helfenstein, Paul] Cornell Univ, Ctr Radiophys & Space Res, Ithaca, NY 14853 USA. [Ingersoll, Andrew P.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. [Jaumann, Ralf] DLR, Inst Planetary Res, Berlin, Germany. [McKay, Christopher P.] NASA, Ames Res Ctr, Mountain View, CA USA. [Nimmo, Francis] Univ Calif Santa Cruz, Dept Earth & Planetary Sci, Santa Cruz, CA 95064 USA. RP Spencer, JR (reprint author), SW Res Inst, Boulder, CO USA. NR 170 TC 61 Z9 61 U1 2 U2 14 PU SPRINGER PI DORDRECHT PA PO BOX 17, 3300 AA DORDRECHT, NETHERLANDS BN 978-1-4020-9216-9 PY 2009 BP 683 EP 724 DI 10.1007/978-1-4020-9217-6_21 D2 10.1007/978-1-4020-9217-6 PG 42 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BMO21 UT WOS:000273026000021 ER PT B AU Seal, DA Buffington, BB AF Seal, David A. Buffington, Brent B. BE Dougherty, MK Esposito, LW Krimigis, SM TI The Cassini Extended Mission SO SATURN FROM CASSINI-HUYGENS LA English DT Article; Book Chapter AB Based on the overwhelming success of the Cassini/Huygens 4-year tour of Saturn from July 2004 to June 2008, NASA Headquarters approved at least two years of extended mission for continued study of the target-rich Saturnian system. After a rigorous phase of science objective definition and trajectory design and analysis, the Cassini project initiated an efficient, scientifically intense and operationally challenging mission phase, including 60 orbits around Saturn. 26 close Titan flybys, and 10 close icy satellite flybys - including seven more flybys of Enceladus. At the conclusion of the 2-year extended mission, substantial operating margins should be present with some fascinating options for further extensions. C1 [Seal, David A.; Buffington, Brent B.] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. RP Seal, DA (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. NR 20 TC 4 Z9 4 U1 0 U2 0 PU SPRINGER PI DORDRECHT PA PO BOX 17, 3300 AA DORDRECHT, NETHERLANDS BN 978-1-4020-9216-9 PY 2009 BP 725 EP 744 DI 10.1007/978-1-4020-9217-6_22 D2 10.1007/978-1-4020-9217-6 PG 20 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BMO21 UT WOS:000273026000022 ER PT J AU Kharuk, VI Ranson, KJ Im, ST Dvinskaya, ML AF Kharuk, Viacheslav I. Ranson, Kenneth J. Im, Sergey T. Dvinskaya, Maria L. TI Response of Pinus sibirica and Larix sibirica to climate change in southern Siberian alpine forest-tundra ecotone SO SCANDINAVIAN JOURNAL OF FOREST RESEARCH LA English DT Article DE Climate change; forest-tundra ecotone; larch; Siberian pine; tree line ID SWEDISH SCANDES; TREE-LINE; HEIGHT GROWTH; SYLVESTRIS; VEGETATION; IMPACTS; 20TH-CENTURY; PERSPECTIVE; MOUNTAINS; RUSSIA AB A warming climate provides competitive advantages to Siberian pine (Pinus sibirica Du Tour) in areas with sufficient precipitation. The warmer temperatures observed in central Siberia over the past three decades appear to have had a noticeable effect on growth of Siberian pine and larch (Larix sibirica Ledeb.) in the south Siberian Mountain forest-tundra ecotone. Larch is more tolerant of harsh climates and exhibits an arboreal growth form, whereas Siberian pine is in krummholz form. Larch also has an advantage at the upper tree limit and in areas with low precipitation. Since the mid-1980s there have been measurable increases in growth increments, stand densification, regeneration propagation into the alpine tundra and transformation of krummholz into arboreal forms. Warming winter temperatures have been sufficient for increased survival of regeneration. Regeneration responded to temperature increase of 1C by migration to areas 10-40 m higher in elevation. Regeneration has propagated into the alpine tundra at the rate of similar to 1.0-2.0 m year-1. Siberian pine and larch regeneration surpassed their upper historical limit by 10-80 m in elevation. While increased tree growth and migration into alpine tundra areas affect the regional carbon balance, it will also decrease albedo, which may increase warming at the regional level. C1 [Kharuk, Viacheslav I.; Im, Sergey T.; Dvinskaya, Maria L.] VN Sukachev Inst Forest, Krasnoyarsk, Russia. [Ranson, Kenneth J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Kharuk, VI (reprint author), VN Sukachev Inst Forest, Krasnoyarsk, Russia. EM kharuk@ksc.krasn.ru RI Ranson, Kenneth/G-2446-2012; Im, Sergei/J-2736-2016 OI Ranson, Kenneth/0000-0003-3806-7270; Im, Sergei/0000-0002-5794-7938 FU Terrestrial Ecology and Cryospheric Sciences Programs and Russian Fund for Fundamental Investigations [06-05-64939] FX This research was supported in part by the NASA Science Mission Directorate, Terrestrial Ecology and Cryospheric Sciences Programs and Russian Fund for Fundamental Investigations No. 06-05-64939. Special thanks to Joanne Howl, DVM, for assisting with final preparation of the manuscript. NR 42 TC 27 Z9 27 U1 2 U2 11 PU TAYLOR & FRANCIS AS PI OSLO PA KARL JOHANS GATE 5, NO-0154 OSLO, NORWAY SN 0282-7581 J9 SCAND J FOREST RES JI Scand. J. Forest Res. PY 2009 VL 24 IS 2 BP 130 EP 139 AR PII 911108538 DI 10.1080/02827580902845823 PG 10 WC Forestry SC Forestry GA 445ER UT WOS:000266033100004 ER PT J AU Liu, Y Chen, D Kahn, RA He, KB AF Liu Yang Chen Dan Kahn, Ralph A. He KeBin TI Review of the applications of Multiangle Imaging SpectroRadiometer to air quality research SO SCIENCE IN CHINA SERIES D-EARTH SCIENCES LA English DT Article DE aerosol remote sensing; MISR; multiangle imaging; aerosol optical thickness; particulate matters; PM2.5; PM10; air pollution ID AEROSOL OPTICAL DEPTH; MATTER COMPONENT CONCENTRATIONS; GROUND-LEVEL PM2.5; DUST AEROSOLS; MISR; MODIS; DISTRIBUTIONS; RETRIEVAL; THICKNESS; AERONET AB The Multiangle Imaging SpectroRadiometer (MISR) launched by NASA in late 1999 has a unique multiangle design, which points nine cameras at fixed angles along the satellite flight track and collects reflected solar radiation simultaneously. This design allows the retrieval of a rich dataset of particle abundance, shape and composition over both land and ocean. Some of its capabilities have not been seen by any currently operating satellite aerosol sensors. Since MISR is sensitive to fine particles, it provides a new data source to study the spatial and temporal characteristics of air quality over large geographical regions. We first briefly introduce the MISR instrument, the retrieval and structure of MISR aerosol data, and then review the applications of MISR aerosol data in various aspects of air quality research since its launch. These include the spatial distributions of particle pollution events such as dust storms, wild fires, and urban pollution. Because of the high quality of MISR aerosol data, they can be used as quantitative indicators of particle pollution levels. We review the current modeling studies of surface level particle concentrations. Next, we introduce research results using MISR's advanced data such as the plume heights, and particle microphysical properties. In the discussion, we compare MISR research with current MODIS research to the best of our ability as MODIS data have been more extensively explored by the Chinese scientific community. Finally, we summarize the advantages and disadvantages of MISR data related to its applications to the air quality research. Given the highly quantitative measurements and comprehensive aerosol information MISR can provide, we believe that it will provide great values to advance our understanding of the particle air pollution in China. C1 [Chen Dan; He KeBin] Tsinghua Univ, Dept Environm Engn & Sci, Beijing 100084, Peoples R China. [Liu Yang] Harvard Univ, Sch Publ Hlth, Boston, MA 02215 USA. [Kahn, Ralph A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP He, KB (reprint author), Tsinghua Univ, Dept Environm Engn & Sci, Beijing 100084, Peoples R China. EM hekb@tsinghua.edu.cn RI Kahn, Ralph/D-5371-2012; Chen, Dan/R-4486-2016 OI Kahn, Ralph/0000-0002-5234-6359; FU Harvard-EPA Center on Particle Health Effects [R-827353, R-832416]; NASA's Climate and Radiation Research and Analysis Program; National High Technology Research and Development Program of China [2006AA06A305] FX Supported by Harvard-EPA Center on Particle Health Effects (Grant Nos. R-827353 and R-832416), NASA's Climate and Radiation Research and Analysis Program, the EOS-MISR Instrument Project and the National High Technology Research and Development Program of China (Grant No. 2006AA06A305). NR 61 TC 9 Z9 9 U1 2 U2 13 PU SCIENCE PRESS PI BEIJING PA 16 DONGHUANGCHENGGEN NORTH ST, BEIJING 100717, PEOPLES R CHINA SN 1006-9313 J9 SCI CHINA SER D JI Sci. China Ser. D-Earth Sci. PD JAN PY 2009 VL 52 IS 1 BP 132 EP 144 DI 10.1007/s11430-008-0149-6 PG 13 WC Geosciences, Multidisciplinary SC Geology GA 429XI UT WOS:000264953000013 ER PT S AU Normand, E Grant, K Ioup, E Sample, J AF Normand, Eric Grant, Kevin Ioup, Elias Sample, John BE Winslett, M TI Improving Relation Extraction by Exploiting Properties of the Target Relation SO SCIENTIFIC AND STATISTICAL DATABASE MANAGEMENT, PROCEEDINGS SE Lecture Notes in Computer Science LA English DT Proceedings Paper CT 21st International Conference on Scientific and Statistical Database Management CY JUN 02-04, 2009 CL New Orleans, LA SP LATG, Diamond Data Syst, Sun Microsyst, NOVACES, Univ New Orleans AB In this paper we demonstrate and quantify the advantage gained by allowing relation extraction algorithms to make use of information about the cardinality of the target, relation. The two algorithms presented herein differ only in their assumption about the nature of the target relation (one-to-many or many-to-many). The algorithms are tested on the same relation to show the degree of advantage gained by their differing assumptions. Comparison of the performance of the two algorithms oil a one-to-many domain demonstrates the existence of several, previously undocumented behaviors which can he used to improve the performance of relation extraction algorithms. The first is a distinct, inverted u-shape in the initial portion of the recall Curve of the many-to-many algorithm. The second is that, as the number of seeds increases, the rate of improvement of the two algorithms descreases to approach the rate at which new information is added via the seeds. C1 [Normand, Eric; Grant, Kevin; Ioup, Elias; Sample, John] USN, Res Lab, Stennis Space Ctr, Stennis Space Ctr, MS 39529 USA. RP Normand, E (reprint author), USN, Res Lab, Stennis Space Ctr, Stennis Space Ctr, MS 39529 USA. EM enormand@nrlssc.navy.mil; kevin.grant.ctr@nrlssc.navy.mil; eioup@nrlssc.navy.mil; john.sample@nrlssc.navy.mil NR 14 TC 0 Z9 0 U1 0 U2 0 PU SPRINGER-VERLAG BERLIN PI BERLIN PA HEIDELBERGER PLATZ 3, D-14197 BERLIN, GERMANY SN 0302-9743 BN 978-3-642-02278-4 J9 LECT NOTES COMPUT SC PY 2009 VL 5566 BP 553 EP 561 PG 9 WC Computer Science, Information Systems; Computer Science, Theory & Methods SC Computer Science GA BKL72 UT WOS:000268444900037 ER PT B AU Wang, TJ Ofman, L Davila, JM AF Wang, T. J. Ofman, L. Davila, J. M. BE Lites, B Cheung, M Magara, T Mariska, J Reeves, K TI Hinode/EIS Observations of Propagating Slow Magnetoacoustic Waves in a Coronal Loop SO SECOND HINODE SCIENCE MEETING: BEYOND DISCOVERY-TOWARD UNDERSTANDING SE Astronomical Society of the Pacific Conference Series LA English DT Proceedings Paper CT 2nd Hinode Science Meeting CY SEP 29-OCT 03, 2008 CL Natl Ctr Atmospher Res, Ctr Green Campus, Boulder, CO HO Natl Ctr Atmospher Res, Ctr Green Campus ID OSCILLATIONS; TRACE AB We present the first Hinode/EIS observations of 5 min quasi-periodic oscillations detected in the transition region and corona at the footpoint of a coronal loop. The oscillations are characterized by a series of wave packets with nearly constant period, typically persisting for 4-6 cycles. There is an in-phase relation between Doppler shift and intensity oscillations, indicating upwardly propagating slow magnetoacoustic waves in the loop. We find that the oscillations detected in the five coronal lines are highly correlated, and the amplitude decreases with increasing temperature. These oscillations may be caused by the leakage of the photospheric p-modes through the chromosphere and transition region into the corona, which has been suggested as the source for intensity oscillations previously observed by TRACE. The temperature dependence of the oscillation amplitudes can be explained by damping of the waves traveling along the loop with multithread structure near the footpoint. C1 [Wang, T. J.; Ofman, L.] Catholic Univ Amer, Dept Phys, Code 671,Bldg 21-RM 177B, Greenbelt, MD 20770 USA. [Wang, T. J.; Ofman, L.; Davila, J. M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20770 USA. RP Wang, TJ (reprint author), Catholic Univ Amer, Dept Phys, Code 671,Bldg 21-RM 177B, Greenbelt, MD 20770 USA. EM wangtj@helio.gsfc.nasa.gov FU NRL [NO0173-06-1-G033] FX Hinode is a Japanese mission developed and launched by ISAS/JAXA in partnership with NAOJ, NASA, and STFC (UK). The work of LO and TJW was supported by NRL grant NO0173-06-1-G033. NR 9 TC 1 Z9 1 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 978-1-58381-710-0 J9 ASTR SOC P PY 2009 VL 415 BP 28 EP + PG 2 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BQL19 UT WOS:000281239000005 ER PT B AU Kitiashvili, I Jacoutot, L Kosovichev, A Wray, A Mansour, N AF Kitiashvili, Irina Jacoutot, Laetitia Kosovichev, Alexander Wray, Alan Mansour, Nagi BE Lites, B Cheung, M Magara, T Mariska, J Reeves, K TI Realistic Numerical Modeling of Solar Magnetoconvection and Oscillations SO SECOND HINODE SCIENCE MEETING: BEYOND DISCOVERY-TOWARD UNDERSTANDING SE Astronomical Society of the Pacific Conference Series LA English DT Proceedings Paper CT 2nd Hinode Science Meeting CY SEP 29-OCT 03, 2008 CL Natl Ctr Atmospher Res, Ctr Green Campus, Boulder, CO HO Natl Ctr Atmospher Res, Ctr Green Campus ID MAGNETIC-FIELDS; P-MODES; CONVECTION; EXCITATION; MISSION AB We have developed 3D, compressible, non-linear radiative MHD simulations to study the influence of magnetic fields of various strengths and geometries on the turbulent convective cells and on the excitation mechanisms of the acoustic oscillations. The results reveal substantial changes of the granulation structure with increased magnetic field, and a frequency-dependent reduction in the oscillation power. These simulation results reproduce the enhanced high-frequency acoustic emission observed at the boundaries of active region ("acoustic halo" phenomenon). In the presence of inclined magnetic field the solar convection develops filamentary structure with flows concentrated along magnetic filaments, and also exhibits behavior of running magnetoconvective waves, resembling recent observations of the sunspot penumbra dynamics from Hinode/SOT. C1 [Kitiashvili, Irina; Jacoutot, Laetitia] Stanford Univ, Ctr Turbulence Res, 488 Escandido Mall, Stanford, CA 94305 USA. [Kosovichev, Alexander; Wray, Alan] Stanford Univ, HEPL, Stanford, CA 94305 USA. [Mansour, Nagi] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Kitiashvili, I (reprint author), Stanford Univ, Ctr Turbulence Res, 488 Escandido Mall, Stanford, CA 94305 USA. EM irinasun@stanford.edu; sasha@sun.stanford.edu NR 11 TC 0 Z9 0 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 978-1-58381-710-0 J9 ASTR SOC P PY 2009 VL 415 BP 83 EP + PG 2 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BQL19 UT WOS:000281239000016 ER PT B AU Straus, T Fleck, B Jefferies, SM McIntosh, SW Severino, G Steffen, M Tarbell, TD AF Straus, Thomas Fleck, Bernhard Jefferies, Stuart M. McIntosh, Scott W. Severino, Giuseppe Steffen, Matthias Tarbell, Theodore D. BE Lites, B Cheung, M Magara, T Mariska, J Reeves, K TI On the Role of Acoustic-Gravity Waves in the Energetics of the Solar Atmosphere SO SECOND HINODE SCIENCE MEETING: BEYOND DISCOVERY-TOWARD UNDERSTANDING SE Astronomical Society of the Pacific Conference Series LA English DT Proceedings Paper CT 2nd Hinode Science Meeting CY SEP 29-OCT 03, 2008 CL Natl Ctr Atmospher Res, Ctr Green Campus, Boulder, CO HO Natl Ctr Atmospher Res, Ctr Green Campus ID CHROMOSPHERE; FLUX AB In a recent paper (Straus et al. 2008) we determined the energy flux of internal gravity waves in the lower solar atmosphere using a combination of 3D numerical simulations and observations obtained with the IBIS instrument operated at the Dunn Solar Telescope and the Michelson Doppler Imager (MDI) on SOHO. In this paper we extend these studies using coordinated observations from SOT/NFI and SOT/SP on Hinode and MDI. The new measurements confirm that gravity waves are the dominant phenomenon in the quiet middle/upper photosphere and that they transport more mechanical energy than the high-frequency (> 5 mHz) acoustic waves, even though we find an acoustic flux 3-5 times larger than the upper limit estimate of Possum and Carlsson (2005). It therefore appears justified to reconsider the significance of (non-M)HD waves for the energy balance of the solar chromosphere. C1 [Straus, Thomas; Severino, Giuseppe] Osserv Astron Capodimonte, INAF, Via Moiariello 16, I-80131 Naples, Italy. [Fleck, Bernhard] NASA, Goddard Space Flight Ctr, ESA Sci Operat Dept, Greenbelt, MD 20771 USA. [Jefferies, Stuart M.] Univ Hawaii, Inst Astron, Pukalani, HI 96768 USA. [McIntosh, Scott W.] High Altitude Observ, Boulder, CO 80307 USA. [Steffen, Matthias] Astrophys Inst Potsdam, D-14482 Potsdam, Germany. [Tarbell, Theodore D.] Lockheed Martin Solar & Astrophys Lab, Palo Alto, CA 94304 USA. RP Straus, T (reprint author), Osserv Astron Capodimonte, INAF, Via Moiariello 16, I-80131 Naples, Italy. EM bfleck@esa.nascom.nasa.gov; mscott@ucar.edu; tarbell@lmsal.com RI Fleck, Bernhard/C-9520-2012 NR 11 TC 9 Z9 9 U1 1 U2 1 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 978-1-58381-710-0 J9 ASTR SOC P PY 2009 VL 415 BP 95 EP + PG 2 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BQL19 UT WOS:000281239000019 ER PT B AU Panasenco, O Velli, M AF Panasenco, Olga Velli, Marco BE Lites, B Cheung, M Magara, T Mariska, J Reeves, K TI Plasma Motions in Prominences Observed by Hinode/SOT SO SECOND HINODE SCIENCE MEETING: BEYOND DISCOVERY-TOWARD UNDERSTANDING SE Astronomical Society of the Pacific Conference Series LA English DT Proceedings Paper CT 2nd Hinode Science Meeting CY SEP 29-OCT 03, 2008 CL Natl Ctr Atmospher Res, Ctr Green Campus, Boulder, CO HO Natl Ctr Atmospher Res, Ctr Green Campus ID MAGNETIC-FIELD; INSTABILITY AB We analyze the plasma motions inside prominences observed by Hinode/SOT during 2006-2007 with focus on the two spectacular examples from 25 April 2007 in H alpha line and 30 November 2006 in the CaH line. It is now well-known that most filaments (prominences on the limb) are composed of fine threads of similar dimensions. Recent observations of counter-streaming motions together with oscillations along the threads provide strong evidence that the threads are field aligned. To more correctly interpret the nature of observed downward flows of dense and cool plasma as well as the upward dark flows of less dense plasma, we take into account the geometry of the prominence structures and the viewing angle. Basic plasma physical considerations lead one to conclude that the magnetic field for the SOT observations considered above must be mainly orthogonal to the plane of the sky. C1 [Panasenco, Olga] Helio Res, 5212 Maryland Ave, La Crescenta, CA 91214 USA. [Velli, Marco] Jet Prop Lab, Pasadena, CA USA. RP Panasenco, O (reprint author), Helio Res, 5212 Maryland Ave, La Crescenta, CA 91214 USA. EM OlgaPanasenco@aol.com; velli@arcetri.astro.it NR 10 TC 1 Z9 1 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 978-1-58381-710-0 J9 ASTR SOC P PY 2009 VL 415 BP 196 EP + PG 3 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BQL19 UT WOS:000281239000038 ER PT B AU Klimchuk, JA AF Klimchuk, James A. BE Lites, B Cheung, M Magara, T Mariska, J Reeves, K TI Coronal Loop Models and Those Annoying Observations! (Keynote) SO SECOND HINODE SCIENCE MEETING: BEYOND DISCOVERY-TOWARD UNDERSTANDING SE Astronomical Society of the Pacific Conference Series LA English DT Proceedings Paper CT 2nd Hinode Science Meeting CY SEP 29-OCT 03, 2008 CL Natl Ctr Atmospher Res, Ctr Green Campus, Boulder, CO HO Natl Ctr Atmospher Res, Ctr Green Campus ID ACTIVE-REGION LOOPS; X-RAY; SPECTROSCOPIC OBSERVATIONS; IMAGING SPECTROMETER; HOT PLASMA; HINODE; TELESCOPE; EXPLORER; MOTIONS; TRACE AB It was once thought that all coronal loops are in static equilibrium, but observational and modeling developments over the past decade have shown that this is clearly not the case. It is now established that warm (similar to 1 MK) loops observed in the EUV are explainable as bundles of unresolved strands that are heated impulsively by storms of nanoflares. A raging debate concerning the multi-thermal versus isothermal nature of the loops can be reconciled in terms of the duration of the storm. We show that short and long storms produce narrow and broad thermal distributions, respectively. We also examine the possibility that warm loops can be explained with thermal nonequilibrium, a process by which steady heating produces dynamic behavior whenever the heating is highly concentrated near the loop footpoints. We conclude that this is not a viable explanation for monolithic loops under the conditions we have considered, but that it may have application to multi-stranded loops. Serious questions remain, however. C1 NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Klimchuk, JA (reprint author), NASA, Goddard Space Flight Ctr, Code 671, Greenbelt, MD 20771 USA. EM James.A.Klimchuk@nasa.gov RI Klimchuk, James/D-1041-2012 OI Klimchuk, James/0000-0003-2255-0305 NR 36 TC 42 Z9 42 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 978-1-58381-710-0 J9 ASTR SOC P PY 2009 VL 415 BP 221 EP 233 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BQL19 UT WOS:000281239000043 ER PT B AU Reale, F Klimchuk, JA Parenti, S Testa, P AF Reale, Fabio Klimchuk, James A. Parenti, Susanna Testa, Paola BE Lites, B Cheung, M Magara, T Mariska, J Reeves, K TI XRT Detection of Hot Plasma in Active Regions and Nanoflare Heating SO SECOND HINODE SCIENCE MEETING: BEYOND DISCOVERY-TOWARD UNDERSTANDING SE Astronomical Society of the Pacific Conference Series LA English DT Proceedings Paper CT 2nd Hinode Science Meeting CY SEP 29-OCT 03, 2008 CL Natl Ctr Atmospher Res, Ctr Green Campus, Boulder, CO HO Natl Ctr Atmospher Res, Ctr Green Campus ID CORONA; LOOPS AB Nanoflares occurring in sub-resolution strands have been long invoked as strong candidates for the heating of active region (AR) coronal loops. However, the frequent occurrence of nanoflares requires the steady presence of flare-hot plasma in the active region, which has been difficult to detect so far. We report on the analysis of multi-filter Hinode/XRT observations of an active region, which may show the widespread presence of 10 MK plasma. C1 [Reale, Fabio] Univ Palermo, Dipartimento Sci Fis & Astron, Sez Astron, Piazza Parlamento 1, I-90134 Palermo, Italy. [Reale, Fabio] Osserv Astron Palermo, INAF, I-90134 Palermo, Italy. [Klimchuk, James A.] NASA, Goddard Space Flight Ctr, Solar Phys Lab, Greenbelt, MD 20771 USA. [Parenti, Susanna] Observ Royal Belgique, B-1180 Brussels, Belgium. [Testa, Paola] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Reale, F (reprint author), Univ Palermo, Dipartimento Sci Fis & Astron, Sez Astron, Piazza Parlamento 1, I-90134 Palermo, Italy. EM reale@astropa.unipa.it; James.A.Klimchuk@nasa.gov; ptesta@cfa.harvard.edu RI Klimchuk, James/D-1041-2012 OI Klimchuk, James/0000-0003-2255-0305 FU Italian Ministero dell'Universita e Ricerca and Agenzia Spaziale Italiana (ASI) [I/015/07/0]; NASA [NNM07AA02C]; Belgian Federal Science Policy Office; International Space Science Institute FX 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). FR acknowledges support from Italian Ministero dellUniversita e Ricerca and Agenzia Spaziale Italiana (ASI) contract I/015/07/0. US members of the XRT team are supported by NASA contract NNM07AA02C to SAO. SP acknowledge the support from the Belgian Federal Science Policy Office through the ESA-PRODEX program. This work was partially supported by the International Space Science Institute in the framework of an international working team. NR 9 TC 0 Z9 0 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 978-1-58381-710-0 J9 ASTR SOC P PY 2009 VL 415 BP 256 EP + PG 2 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BQL19 UT WOS:000281239000048 ER PT B AU Del Zanna, G Bradshaw, SJ AF Del Zanna, G. Bradshaw, S. J. BE Lites, B Cheung, M Magara, T Mariska, J Reeves, K TI Coronal Loops: New Insights from EIS Observations SO SECOND HINODE SCIENCE MEETING: BEYOND DISCOVERY-TOWARD UNDERSTANDING SE Astronomical Society of the Pacific Conference Series LA English DT Proceedings Paper CT 2nd Hinode Science Meeting CY SEP 29-OCT 03, 2008 CL Natl Ctr Atmospher Res, Ctr Green Campus, Boulder, CO HO Natl Ctr Atmospher Res, Ctr Green Campus ID HINODE EIS AB Multi-instrument observations of coronal loops of different active regions have been studied. The general features discussed in Del Zanna (2003) and Del Zanna and Mason (2003) based on SOHO/CDS are confirmed. Hinnode/EIS high-cadence observations clearly show how dynamic loops are at all temperatures. This clearly reflects the fast changes in the photospheric magnetic fields measured by SOT over a minute timescale. Despite that, persistent patterns are present. In particular, the pattern of Doppler shifts and non-thermal widths, found for the first time in NOAA 10926 (cf. Del Zanna 2007, 2008), is actually a common feature in all active regions. It is likely that the majority of cool (0.5-1 MK) loops are observed during their radiatively cooling phase. C1 [Del Zanna, G.] Univ Coll London, Mullard Space Sci Lab, Holmbury St Mary, Dorking RH5 6NT, Surrey, England. [Del Zanna, G.] DAMPT, Ctr Math Sci, Cambridge CB3 0WA, England. [Bradshaw, S. J.] NASA, Goddard Space Flight Ctr, Solar Phys Lab, Greenbelt, MD 20771 USA. [Bradshaw, S. J.] George Mason Univ, Dept Comp & Data Sci, Fairfax, VA 22030 USA. RP Del Zanna, G (reprint author), Univ Coll London, Mullard Space Sci Lab, Holmbury St Mary, Dorking RH5 6NT, Surrey, England. EM gdz@mssl.ucl.ac.uk NR 6 TC 2 Z9 2 U1 2 U2 2 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 978-1-58381-710-0 J9 ASTR SOC P PY 2009 VL 415 BP 264 EP + PG 2 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BQL19 UT WOS:000281239000050 ER PT B AU McIntosh, SW Burkepile, J Leamon, RJ AF McIntosh, Scott W. Burkepile, Joan Leamon, Robert J. BE Lites, B Cheung, M Magara, T Mariska, J Reeves, K TI More of the Inconvenient Truth About Coronal Dimmings SO SECOND HINODE SCIENCE MEETING: BEYOND DISCOVERY-TOWARD UNDERSTANDING SE Astronomical Society of the Pacific Conference Series LA English DT Proceedings Paper CT 2nd Hinode Science Meeting CY SEP 29-OCT 03, 2008 CL Natl Ctr Atmospher Res, Ctr Green Campus, Boulder, CO HO Natl Ctr Atmospher Res, Ctr Green Campus ID MASS EJECTIONS; HINODE; MISSION AB We continue the investigation of a CME-driven coronal dimming from December 14 2006 using unique high resolution imaging of the chromosphere and corona from the Hinode spacecraft. Over the course of the dimming event we observe the dynamic increase of non-thermal line broadening of multiple emission lines as the CME is released and the corona opens; reaching levels seen in coronal holes. As the corona begins to close, refill and brighten, we see a reduction of the non-thermal broadening towards the pre-eruption level. The dynamic evolution of non-thermal broadening is consistent with the expected change of Alfven wave amplitudes in the magnetically open rarefied dimming region, compared to the dense closed corona prior to the CME. The presented data reinforce the belief that coronal dimmings must be temporary sources of the fast solar wind. It is unclear if such a rapid transition in the thermodynamics of the corona to a solar wind state has an effect on the CME itself. C1 [McIntosh, Scott W.; Burkepile, Joan] Natl Ctr Atmospher Res, High Altitude Observ, POB 3000, Boulder, CO 80307 USA. [Leamon, Robert J.] Adnet Syst Inc, NASA Goddard Space Flight Ctr, 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; iguana@ucar.edu NR 12 TC 1 Z9 1 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 978-1-58381-710-0 J9 ASTR SOC P PY 2009 VL 415 BP 393 EP + PG 2 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BQL19 UT WOS:000281239000077 ER PT B AU Wang, TJ Sui, L Qiu, J AF Wang, T. J. Sui, L. Qiu, J. BE Lites, B Cheung, M Magara, T Mariska, J Reeves, K TI Direct Observation of High-Speed Reconnection Outflows With SOHO/SUMER, TRACE and RHESSI SO SECOND HINODE SCIENCE MEETING: BEYOND DISCOVERY-TOWARD UNDERSTANDING SE Astronomical Society of the Pacific Conference Series LA English DT Proceedings Paper CT 2nd Hinode Science Meeting CY SEP 29-OCT 03, 2008 CL Natl Ctr Atmospher Res, Ctr Green Campus, Boulder, CO HO Natl Ctr Atmospher Res, Ctr Green Campus ID MAGNETIC RECONNECTION; SOLAR-FLARES AB Spectroscopic observations of a solar limb flare recorded by SUMER on SOHO reveal, for the first time, hot fast magnetic reconnection outflows in the corona. The observations from TRACE and RHESSI allow us to determine the location of magnetic reconnection region. We find that as the reconnection site rises across the SUMER spectrometer slit, significant blue- and red-shift signatures are observed in the Fe XIX line, reflecting upflows and downflows of hot plasma jets, respectively. With the projection effect corrected, the measured outflow speed is between about 900-3500 km/s, consistent with theoretical predictions. This study provides an important guidance to the future observation with Hinode/EIS. C1 [Wang, T. J.; Sui, L.] Catholic Univ Amer, Dept Phys, Code 671, Greenbelt, MD 20770 USA. [Wang, T. J.; Sui, L.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Qiu, J.] Montana State Univ, Dept Phys, Bozeman, MT 59717 USA. RP Wang, TJ (reprint author), Catholic Univ Amer, Dept Phys, Code 671, Greenbelt, MD 20770 USA. EM wangtj@helio.gsfc.nasa.gov NR 5 TC 1 Z9 1 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 978-1-58381-710-0 J9 ASTR SOC P PY 2009 VL 415 BP 447 EP + PG 2 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BQL19 UT WOS:000281239000087 ER PT S AU Eggert, J Ryan, SJ Ramesh, KT Funk, D Proud, W AF Eggert, J. Ryan, S. J. Ramesh, K. T. Funk, D. Proud, W. G. BE Elert, ML Buttler, WT Furnish, MD Anderson, WW Proud, WG TI TOWN HALL MEETING - SCCM 2009 SO SHOCK COMPRESSION OF CONDENSED MATTER - 2009, PTS 1 AND 2 SE AIP Conference Proceedings LA English DT Proceedings Paper CT 16th Conference of the American-Physical-Society-Topical-Group on Shock Compression of Condensed Matter CY JUN 28-JUL 03, 2009 CL Nashville, TN SP Amer Phys Soc, Topical Grp DE communication satellites; nanoscale materials and structures; metrology AB The following article contains the summary of the discussion held at the Shock Compression of Condensed Matter Town Hall Meeting. This was held on Tuesday afternoon of the meeting and attracted 100+ attendees. This meeting, chaired by John Eggert, was planned to introduce challenges in selected topics relevant to shock wave science. The three subjects and speakers were: space research introduced by Shannon Ryan, nanotechnology presented by Kaliat T. Ramesh, and compression tools delivered by Dave Funk. After each presentation there were a number of questions. C1 [Eggert, J.] Lawrence Livermore Natl Lab, POB 808, Livermore, CA 94551 USA. [Ryan, S. J.] HITF, NASA Johnson Space Ctr, Houston, TX USA. [Ramesh, K. T.] Johns Hopkins Univ, Dept Mech Engn, Baltimore, MD 21218 USA. [Funk, D.] Los Alamos Natl Lab, Los Alamos, NM 87545 USA. [Proud, W. G.] Fracture & Shock Phys Grp, Cavendish Lab, Cambridge CB30HE, England. RP Eggert, J (reprint author), Lawrence Livermore Natl Lab, POB 808, Livermore, CA 94551 USA. NR 1 TC 0 Z9 0 U1 0 U2 1 PU AMER INST PHYSICS PI MELVILLE PA 2 HUNTINGTON QUADRANGLE, STE 1NO1, MELVILLE, NY 11747-4501 USA SN 0094-243X BN 978-0-7354-0732-9 J9 AIP CONF PROC PY 2009 VL 1195 BP 26 EP + PG 2 WC Physics, Condensed Matter SC Physics GA BOG48 UT WOS:000276574100004 ER PT S AU Ryan, SJ Christiansen, EL Lear, DM AF Ryan, S. J. Christiansen, E. L. Lear, D. M. BE Elert, ML Buttler, WT Furnish, MD Anderson, WW Proud, WG TI DEVELOPMENT OF THE NEXT GENERATION OF METEOROID AND ORBITAL DEBRIS SHIELDS SO SHOCK COMPRESSION OF CONDENSED MATTER - 2009, PTS 1 AND 2 SE AIP Conference Proceedings LA English DT Proceedings Paper CT 16th Conference of the American-Physical-Society-Topical-Group on Shock Compression of Condensed Matter CY JUN 28-JUL 03, 2009 CL Nashville, TN SP Amer Phys Soc, Topical Grp DE Hypervelocity impact; aluminum: foam; penetration ID SPACECRAFT AB The novel structure of metallic foams is of interest in the design of next-generation debris shields as it introduces physical mechanisms that are advantageous to hypervelocity impact shielding (e.g. increased fragmentation/melt/vaporization, energy dissipation, etc.). Preliminary investigations have shown improved shielding capability over traditional spacecraft primary structures. In this paper, the results of a current hypervelocity impact test program on metallic open-cell foam core sandwich panels are reported. A preliminary ballistic limit equation has been derived from the experimental results, and is presented in a form suitable for implementation in risk assessment software codes. C1 [Ryan, S. J.] USRA Lunar & Planetary Inst, 3600 Bay Area Blvd, Houston, TX 77058 USA. [Christiansen, E. L.; Lear, D. M.] NASA, Johnson Space Ctr, Houston, TX 77058 USA. RP Ryan, SJ (reprint author), USRA Lunar & Planetary Inst, 3600 Bay Area Blvd, Houston, TX 77058 USA. NR 10 TC 1 Z9 1 U1 0 U2 0 PU AMER INST PHYSICS PI MELVILLE PA 2 HUNTINGTON QUADRANGLE, STE 1NO1, MELVILLE, NY 11747-4501 USA SN 0094-243X BN 978-0-7354-0732-9 J9 AIP CONF PROC PY 2009 VL 1195 BP 1417 EP + PG 2 WC Physics, Condensed Matter SC Physics GA BOG48 UT WOS:000276574100334 ER PT S AU Sankrit, R Williams, BJ Borkowski, KJ Raymond, JC Gaetz, TJ Blair, WP Ghavamian, P Long, KS Reynolds, SP AF Sankrit, Ravi Williams, Brian J. Borkowski, Kazimierz J. Raymond, John C. Gaetz, Terrance J. Blair, William P. Ghavamian, Parviz Long, Knox S. Reynolds, Stephen P. BE Ao, X Burrows, R Zank, GP TI Dust Destruction in a Nonradiative Shock in the Cygnus Loop Supernova Remnant SO SHOCK WAVES IN SPACE AND ASTROPHYSICAL ENVIRONMENTS SE AIP Conference Proceedings LA English DT Proceedings Paper CT 8th Annual International Astrophysics Conference CY MAY 01-07, 2009 CL Kona, HI SP Univ Alabama Huntsville, Ctr Space Plasma & Aeronom Res DE Dust; Shocks; Supernova Remnants ID LARGE-MAGELLANIC-CLOUD; SPECTRA AB We present 24 mu m and 70 mu m images of a non-radiative shock in the Cygnus Loop supernova remnant, obtained with the Multiband Imaging Photometer on board the Spitzer Space Telescope. The observed emission is from dust grains heated in the post-shock region. The 70 mu m to 24 mu m flux ratio depends on the dust heating and the dust destruction rates, and thereby it is a sensitive tracer of the gas density and temperature in the shocked plasma. We model the dust emission and grain destruction in the post-shock flow, and find that the observed 70 mu m to 24 mu m flux ratios are produced for post-shock densities, n(H) similar to 2.0 cm(-3) and electron temperatures of about 0.20 keV. We find that about 35% of the dust has been destroyed in the shock, and that non-thermal sputtering (i.e. sputtering due to bulk motion of the grains relative to the gas) contributes significantly to the dust destruction. C1 [Sankrit, Ravi] NASA, SOFIA, Ames Res Ctr, M-S 211-3, Moffett Field, CA 94041 USA. [Williams, Brian J.; Borkowski, Kazimierz J.; Reynolds, Stephen P.] North Carolina State Univ, Raleigh, NC 27695 USA. [Raymond, John C.; Gaetz, Terrance J.] Smithsonian Astrophys Observ, Cambridge, MA USA. [Blair, William P.] Johns Hopkins Univ, Baltimore, MD 21218 USA. [Ghavamian, Parviz; Long, Knox S.] STScI, Baltimore, MD USA. RP Sankrit, R (reprint author), NASA, SOFIA, Ames Res Ctr, M-S 211-3, Moffett Field, CA 94041 USA. FU JPL [1278412]; SOFIA Science Center/USRA FX This work was supported in part by JPL Award 1278412 to the University of California, Berkeley and North Carolina State University. RS acknowledges support from the SOFIA Science Center/USRA. NR 10 TC 0 Z9 0 U1 0 U2 0 PU AMER INST PHYSICS PI MELVILLE PA 2 HUNTINGTON QUADRANGLE, STE 1NO1, MELVILLE, NY 11747-4501 USA SN 0094-243X BN 978-0-7354-0724-4 J9 AIP CONF PROC PY 2009 VL 1183 BP 95 EP + PG 2 WC Astronomy & Astrophysics; Physics, Applied SC Astronomy & Astrophysics; Physics GA BPZ45 UT WOS:000280435400012 ER PT B AU Liou, MS Chang, CH Chen, H Hu, JJ AF Liou, M. -S. Chang, C. -H. Chen, H. Hu, J. -J. BE Hannemann, K Seiler, F TI Numerical study of shock-driven deformation of interfaces SO SHOCK WAVES, VOL 2, PROCEEDINGS LA English DT Proceedings Paper CT 26th International Symposium on Shock Waves CY JUL 15-20, 2007 CL Gottingen, GERMANY SP German Aerosp Ctr, French German Res Inst St Louis ID 2-PHASE FLOW; WAVES AB We employ AUSM(+)-up to obtain numerical results for studying the deformation of a droplet and an air bubble impacted initially by a passing shock wave, which triggers sequences of all enormously complicated flowfield. Multiplicate shock and rarefaction waves, and contact/slip surfaces have developed and interacted with each other, resulting in incredibly fine structures. Further analysis of the results yields useful insight into the behavior of interface dynamics, providing a new light oil the path to understanding of droplet breakup and jet formation. C1 [Liou, M. -S.] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. [Chang, C. -H.] Univ Calif, Ctr Risk Stud & Safety, Goleta, CA 93117 USA. [Chen, H.] Leader Univ, Tainan 70970, Taiwan. [Hu, J. -J.] Shu Te Univ, Kaohsiung 82445, Taiwan. RP Liou, MS (reprint author), NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. NR 16 TC 0 Z9 0 U1 0 U2 0 PU SPRINGER-VERLAG BERLIN PI BERLIN PA HEIDELBERGER PLATZ 3, D-14197 BERLIN, GERMANY BN 978-3-540-85180-6 PY 2009 BP 919 EP + DI 10.1007/978-3-540-85181-3_20 PG 2 WC Engineering, Mechanical; Mechanics; Physics, Applied; Physics, Multidisciplinary SC Engineering; Mechanics; Physics GA BKZ48 UT WOS:000269687500020 ER PT S AU Spry, DJ Neudeck, PG Chen, LY Beheim, GM Okojie, RS Chang, CW Meredith, RD Ferrier, TL Evans, LJ AF Spry, David J. Neudeck, Philip G. Chen, Liang-Yu Beheim, Glenn M. Okojie, Robert S. Chang, Carl W. Meredith, Roger D. Ferrier, Terry L. Evans, Laura J. BE Suzuki, A Okumura, H Kimoto, T Fuyuki, T Fukuda, K Nishizawa, S TI Fabrication and Testing of 6H-SiC JFETs for Prolonged 500 degrees C Operation in Air Ambient SO SILICON CARBIDE AND RELATED MATERIALS 2007, PTS 1 AND 2 SE Materials Science Forum LA English DT Proceedings Paper CT 12th International Conference on Silicon Carbide and Related Materials CY OCT 14-19, 2007 CL Otsu, JAPAN SP Japan Soc Appl Phys, Assoc Promot Elect, Elect & Informat Engn, Ceram Soc Japan, IEEE EDS, Kansai Chapter, IEEJ, Inst Elect, Informat & Commun Engineers, Japanese Assoc Crystal Growth, Surface Sci Soc Japan, Vacuum Soc Japan DE 6H-SiC; JFET; Junction Field Effect; Transistor; Durability; Reliability; High Temperature; Amplifier; Differential Amplifier; Packaging AB This paper reports on the fabrication and testing of 6H-SiC junction field effect transistors (JFETs) and a simple differential amplifier integrated circuit that have demonstrated 2000 hours of electrical operation at 500 degrees C without degradation. The high-temperature ohmic contacts, dielectric passivation, and packaging technology that enabled such 500 degrees C durability are briefly described. Key JFET parameters of threshold voltage, on-state resistance, transconductance, and on-state current, as well as the gain of the differential amplifier integrated circuit, exhibited less than 7% change over the first 2000 hours of 500 degrees C operational testing. C1 [Spry, David J.; Chen, Liang-Yu] NASA Glenn, OAI, 21000 Brookpk Rd,MS 77-1, Cleveland, OH 44135 USA. [Neudeck, Philip G.; Beheim, Glenn M.; Okojie, Robert S.; Meredith, Roger D.; Ferrier, Terry L.; Evans, Laura J.] NASA Glenn Res Ctr, Cleveland, OH 44135 USA. [Chang, Carl W.] ASRC Aerosp Corp, Cleveland, OH 44135 USA. RP Spry, DJ (reprint author), NASA Glenn, OAI, 21000 Brookpk Rd,MS 77-1, Cleveland, OH 44135 USA. EM David.J.Spry@nasa.gov; Philip.G.Neudeck@nasa.gov; Liangyu.Chen@grc.nasa.gov FU NASA Aeronautics Research Mission Directorate; Fundamental Aeronautics Programs under the Integrated Vehicle Health Management, Subsonic Fixed Wing; Supersonics Projects; NASA FX This work is presently funded by the NASA Aeronautics Research Mission Directorate in both the Aviation Safety and Fundamental Aeronautics Programs under the Integrated Vehicle Health Management, Subsonic Fixed Wing, and Supersonics Projects. Prior-year NASA funding for this work included the Glennan Microsystems Initiative, Ultra Efficient Engine Technology, Propulsion 21, and NASA electronics Parts and Packaging programs. Work was carried out by NASA Glenn Research Center with assistance of D. Lukco, A. Trunek, D. Androjna, K. Laster, J. Gonzalez, R. Lotenero, M. Mrdenovich, B. Osborn, G. Hunter, and L. Matus. NR 6 TC 6 Z9 6 U1 0 U2 0 PU TRANS TECH PUBLICATIONS LTD PI DURNTEN-ZURICH PA KREUZSTRASSE 10, 8635 DURNTEN-ZURICH, SWITZERLAND SN 0255-5476 J9 MATER SCI FORUM PY 2009 VL 600-603 BP 1079 EP + PN 1-2 PG 2 WC Materials Science, Ceramics; Materials Science, Multidisciplinary SC Materials Science GA BIX26 UT WOS:000263555300258 ER PT S AU Patil, A Fu, XA Neudeck, P Beheim, G Mehregany, M Garverick, S AF Patil, Amita Fu, Xiao-an Neudeck, Philip Beheim, Glenn Mehregany, Mehran Garverick, Steven BE Suzuki, A Okumura, H Kimoto, T Fuyuki, T Fukuda, K Nishizawa, S TI Silicon Carbide Differential Amplifiers for High-Temperature Sensing SO SILICON CARBIDE AND RELATED MATERIALS 2007, PTS 1 AND 2 SE Materials Science Forum LA English DT Proceedings Paper CT 12th International Conference on Silicon Carbide and Related Materials CY OCT 14-19, 2007 CL Otsu, JAPAN SP Japan Soc Appl Phys, Assoc Promot Elect, Elect & Informat Engn, Ceram Soc Japan, IEEE EDS, Kansai Chapter, IEEJ, Inst Elect, Informat & Commun Engineers, Japanese Assoc Crystal Growth, Surface Sci Soc Japan, Vacuum Soc Japan DE Junction field effect transistors; silicon carbide electronics; high-temperature electronics; sensor interface circuits; differential amplifiers AB This paper presents silicon carbide sensor interface circuits and techniques for MEMS-based sensors operating in harsh environments. More specifically, differential amplifiers were constructed using integrated, depletion-mode, n-channel, 6H-SiC JFETs and off-chip passive components. A three-stage voltage amplifier has a differential voltage gain of similar to 50 dB and a gain-bandwidth of similar to 200 kHz at 450 degrees C, as limited by test parasitics. Such an amplifier could be used to amplify the signals produced by a piezoresistive Wheatstone bridge sensor, for example. Design considerations for 6H-SiC JFET transimpedance amplifiers appropriate for capacitance sensing and for frequency readout from a micromechanical resonator are also presented. C1 [Patil, Amita; Fu, Xiao-an; Mehregany, Mehran; Garverick, Steven] Case Western Reserve Univ, Cleveland, OH 44106 USA. [Neudeck, Philip; Beheim, Glenn] NASA Glenn Res Ctr, Cleveland, OH USA. RP Patil, A (reprint author), Case Western Reserve Univ, Cleveland, OH 44106 USA. EM amita.patil@case.edu; xiao-an.fu@case.edu; Philip.G.Neudeck@nasa.gov; glenn.m.beheim@nasa.gov; mehran@case.edu; steven.garverick@case.edu FU DARPA [NBCH1050002]; Glennan Microsystems Initiative and the Integrated Vehicle Health Management Project under the Aviation Safety Program FX This work was supported by DARPA under award #NBCH1050002. Work at NASA Glenn Research Center was supported by the Glennan Microsystems Initiative and the Integrated Vehicle Health Management Project under the Aviation Safety Program. NR 8 TC 5 Z9 5 U1 0 U2 0 PU TRANS TECH PUBLICATIONS LTD PI DURNTEN-ZURICH PA KREUZSTRASSE 10, 8635 DURNTEN-ZURICH, SWITZERLAND SN 0255-5476 J9 MATER SCI FORUM PY 2009 VL 600-603 BP 1083 EP + PN 1-2 PG 2 WC Materials Science, Ceramics; Materials Science, Multidisciplinary SC Materials Science GA BIX26 UT WOS:000263555300259 ER PT S AU Fu, XA Patil, A Neudeck, PG Beheim, GM Garverick, SL Mehregany, M AF Fu, Xiao-An Patil, Amita Neudeck, Philip G. Beheim, Glenn M. Garverick, Steven L. Mehregany, Mehran BE Suzuki, A Okumura, H Kimoto, T Fuyuki, T Fukuda, K Nishizawa, S TI 6H-SiC Lateral JFETs for Analog Integrated Circuits SO SILICON CARBIDE AND RELATED MATERIALS 2007, PTS 1 AND 2 SE Materials Science Forum LA English DT Proceedings Paper CT 12th International Conference on Silicon Carbide and Related Materials CY OCT 14-19, 2007 CL Otsu, JAPAN SP Japan Soc Appl Phys, Assoc Promot Elect, Elect & Informat Engn, Ceram Soc Japan, IEEE EDS, Kansai Chapter, IEEJ, Inst Elect, Informat & Commun Engineers, Japanese Assoc Crystal Growth, Surface Sci Soc Japan, Vacuum Soc Japan DE JFET; high temperature electronics; 6H-SiC; device physics; device fabrication ID TEMPERATURE AB This paper reports fabrication and electrical characterization of 6H-SiC n-channel, depletion-mode, junction-field-effect transistors (JFETs) for use in high-temperature analog integrated circuits for sensing and control in propulsion, power systems, and geothermal exploration. Electrical characteristics of the resulting MET devices have been measured across the wafer as a function of temperature, from room temperature to 450 degrees C. The results indicate that the JFETs are suitable for high-gain amplifiers in high-temperature sensor signal processing circuits. C1 [Fu, Xiao-An; Patil, Amita; Garverick, Steven L.; Mehregany, Mehran] Case Western Reserve Univ, Dept Elect Engn & Comp Sci, Cleveland, OH 44106 USA. [Neudeck, Philip G.; Beheim, Glenn M.] NASA Glenn Res Ctr, Cleveland, OH 44135 USA. RP Fu, XA (reprint author), Case Western Reserve Univ, Dept Elect Engn & Comp Sci, Cleveland, OH 44106 USA. EM xxf@case.edu; amita@case.edu; Philip.G.Neudeck@nasa.gov; Glenn.M.Beheim@nasa.gov; steven.garverick@case.edu; mehran@case.edu FU DARPA [NBCH1050002]; Glennan Microsystems Initiative; Integrated Vehicle Health Management Project under the Aviation Safety Program FX The authors would like to thank Mr. David Spry for technical contributions to NASA Glenns SiC electronics research. This work was supported by DARPA under award #NBCH1050002. Work at NASA Glenn Research Center was supported by the Glennan Microsystems Initiative and the Integrated Vehicle Health Management Project under the Aviation Safety Program. NR 7 TC 1 Z9 1 U1 0 U2 0 PU TRANS TECH PUBLICATIONS LTD PI DURNTEN-ZURICH PA KREUZSTRASSE 10, 8635 DURNTEN-ZURICH, SWITZERLAND SN 0255-5476 J9 MATER SCI FORUM PY 2009 VL 600-603 BP 1099 EP + PN 1-2 PG 2 WC Materials Science, Ceramics; Materials Science, Multidisciplinary SC Materials Science GA BIX26 UT WOS:000263555300263 ER PT S AU Neudeck, PG Spry, DJ Trunek, AJ Evans, LJ Chen, LY Hunter, GW Androjna, D AF Neudeck, Philip G. Spry, David J. Trunek, Andrew J. Evans, Laura J. Chen, Liang-Yu Hunter, Gary W. Androjna, Drago BE Suzuki, A Okumura, H Kimoto, T Fuyuki, T Fukuda, K Nishizawa, S TI Hydrogen Gas Sensors Fabricated on Atomically Flat 4H-SiC Webbed Cantilevers SO SILICON CARBIDE AND RELATED MATERIALS 2007, PTS 1 AND 2 SE Materials Science Forum LA English DT Proceedings Paper CT 12th International Conference on Silicon Carbide and Related Materials CY OCT 14-19, 2007 CL Otsu, JAPAN SP Japan Soc Appl Phys, Assoc Promot Elect, Elect & Informat Engn, Ceram Soc Japan, IEEE EDS, Kansai Chapter, IEEJ, Inst Elect, Informat & Commun Engineers, Japanese Assoc Crystal Growth, Surface Sci Soc Japan, Vacuum Soc Japan DE Gas Sensor; Hydrogen; Webbed Cantilevers; Hydrogen Sensor; Atomically Flat; On-axis; Step-free Surface; Schottky Diode; Platinum AB This paper reports on initial results from the first device tested of a "second generation" Pt-SiC Schottky diode hydrogen gas sensor that: 1) resides on the top of atomically flat 4H-SiC webbed cantilevers, 2) has integrated heater resistor, and 3) is bonded and packaged. With proper selection of heater resistor and sensor diode biases, rapid detection of H-2 down to concentrations of 20 ppm was achieved. A stable sensor current gain of 125 +/- 11 standard deviation was demonstrated during 250 hours of cyclic test exposures to 0.5% H-2 and N-2/air. C1 [Neudeck, Philip G.; Evans, Laura J.; Hunter, Gary W.] NASA, Glenn Res Ctr, 21000 Brookpk Rd,MS 77-1, Cleveland, OH 44135 USA. [Spry, David J.; Trunek, Andrew J.; Chen, Liang-Yu] NASA, OAI, Cleveland, OH 44135 USA. [Androjna, Drago] Sierra Lobo Inc, NASA, Cleveland, OH 44135 USA. RP Neudeck, PG (reprint author), NASA, Glenn Res Ctr, 21000 Brookpk Rd,MS 77-1, Cleveland, OH 44135 USA. EM Neudeck@nasa.gov; David.J.Spry@nasa.gov; Gary.W.Hunter@nasa.gov FU NASA Aeronautics Research Mission Directorate in the Fundamental Aeronautics Program, Supersonics Project FX The authors thank J. Xu, M. Artale, P. Lampard, B. Osborn, M. Mrdenovich, G. Beheim, R. Okojie, J. A. Powell, and L. Matus at NASA Glenn Research Center for their assistance. This work was funded by the NASA Aeronautics Research Mission Directorate in the Fundamental Aeronautics Program, Supersonics Project. NR 6 TC 8 Z9 8 U1 0 U2 1 PU TRANS TECH PUBLICATIONS LTD PI DURNTEN-ZURICH PA KREUZSTRASSE 10, 8635 DURNTEN-ZURICH, SWITZERLAND SN 0255-5476 J9 MATER SCI FORUM PY 2009 VL 600-603 BP 1199 EP + PN 1-2 PG 2 WC Materials Science, Ceramics; Materials Science, Multidisciplinary SC Materials Science GA BIX26 UT WOS:000263555300288 ER PT S AU Trunek, AJ Powell, JA Neudeck, PG Mrdenovich, M AF Trunek, A. J. Powell, J. A. Neudeck, P. G. Mrdenovich, M. BE PerezTomas, A Godignon, P Vellvehi, M Brosselard, P TI HCl Etching Behavior on Low-Tilt-Angle and Step-Free 4H-SiC Surfaces SO SILICON CARBIDE AND RELATED MATERIALS 2008 SE Materials Science Forum LA English DT Proceedings Paper CT 7th European Conference on Silicon Carbide and Related Materials CY SEP 07-11, 2008 CL Barcelona, SPAIN SP Minist Educ & Cienc, ACCIO, Generalitat Catalunya, ACREO, Aixtron, Cree Inc, Dow Corning, D plus T Microelect, Ion Beam Serv, SiCED, SiCrystal AG DE HCl etching; on-axis; mesa; cold wall ID CONTROLLED GROWTH; EPITAXIAL-GROWTH; 6H-SIC(0001); HOMOEPITAXY; MESAS AB We report on new observations made, when 4H-SiC, Si-face Substrate mesas, having either low tilt-angle (< 1 degrees) with steps or step-free top surfaces, were exposed to three separate HCl etching conditions for five minutes at temperatures of 1130 degrees C, 1240 degrees C and 1390 degrees C. We observed that HCl was ineffective at 1130 degrees C, as etching was incomplete with abundant surface contamination. At 1240 degrees C. screw dislocations were aggressively etched by HCl, while multiple shallow flat-bottomed etch pits were formed oil step-free mesa surfaces. At 1390 degrees C, step-flow etching dominated as large etch pits were formed at screw dislocations and previously step-free surfaces etched inward from mesa edges to form parallel rows of organized steps. C1 [Trunek, A. J.] OAI, Cleveland, OH 44135 USA. [Powell, J. A.] Est Inc, Cleveland, OH 44135 USA. [Neudeck, P. G.] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. [Mrdenovich, M.] Sierra Lobo, Cleveland, OH 44135 USA. RP Trunek, AJ (reprint author), OAI, MS 77-1,21000 Brookpk Rd, Cleveland, OH 44135 USA. EM andrew.j.trunek@nasa.gov; j.a.powell@nasa.gov NR 8 TC 2 Z9 2 U1 0 U2 0 PU TRANS TECH PUBLICATIONS LTD PI STAFA-ZURICH PA LAUBLSRUTISTR 24, CH-8717 STAFA-ZURICH, SWITZERLAND SN 0255-5476 J9 MATER SCI FORUM PY 2009 VL 615-617 BP 593 EP 596 PG 4 WC Engineering, Electrical & Electronic; Materials Science, Ceramics; Materials Science, Multidisciplinary SC Engineering; Materials Science GA BJH84 UT WOS:000265961100143 ER PT S AU Rowland, LB Wyatt, JL Fronheiser, JA Vert, AV Sandvik, PM Borsa, T Van Zeghbroeck, J Van Zeghbroeck, B Babu, S AF Rowland, L. B. Wyatt, J. L. Fronheiser, J. A. Vert, A. V. Sandvik, P. M. Borsa, T. Van Zeghbroeck, J. Van Zeghbroeck, B. Babu, S. BE PerezTomas, A Godignon, P Vellvehi, M Brosselard, P TI 6H and 4H-SiC Avalanche Photodiodes SO SILICON CARBIDE AND RELATED MATERIALS 2008 SE Materials Science Forum LA English DT Proceedings Paper CT 7th European Conference on Silicon Carbide and Related Materials CY SEP 07-11, 2008 CL Barcelona, SPAIN SP Minist Educ & Cienc, ACCIO, Generalitat Catalunya, ACREO, Aixtron, Cree Inc, Dow Corning, D plus T Microelect, Ion Beam Serv, SiCED, SiCrystal AG DE avalanche photodiode; APD; a-plane; 11-20; photodiode; ultraviolet; sensor AB We report on the fabrication and testing of SiC p-i-n avalanche photodiodes. APDs of 0.25 mm(2) area on a-plane (11 (2) over bar0) 6H-SiC as well as off-axis Si face 6H and 4H-SiC were Successfully fabricated. A beveled mesa was used as edge termination. Recessed windows were formed using reactive ion etching to enhance low-wavelength UV performance. We performed current-voltage tests with and without UV illumination to determine dark current, photocurrent, and gain on selected devices. Dark Current was less than 1 pA at 0.5V(br) on multiple devices. Quantum efficiency of 40% or greater was observed for all orientations and polytypes. C1 [Rowland, L. B.; Wyatt, J. L.] Aymont Technol Inc, Ballston Spa, NY 12020 USA. [Fronheiser, J. A.; Vert, A. V.; Sandvik, P. M.] GE Global Res, Niskayuna, NY 12309 USA. [Borsa, T.; Van Zeghbroeck, J.; Van Zeghbroeck, B.] Univ Colorado, Boulder, CO 80301 USA. [Babu, S.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Rowland, LB (reprint author), Aymont Technol Inc, 30 Saratoga Ave,Suite 6H, Ballston Spa, NY 12020 USA. EM rowland@aymont.com RI Rowland, Larry/C-4487-2008 NR 8 TC 2 Z9 2 U1 0 U2 2 PU TRANS TECH PUBLICATIONS LTD PI STAFA-ZURICH PA LAUBLSRUTISTR 24, CH-8717 STAFA-ZURICH, SWITZERLAND SN 0255-5476 J9 MATER SCI FORUM PY 2009 VL 615-617 BP 869 EP 872 PG 4 WC Engineering, Electrical & Electronic; Materials Science, Ceramics; Materials Science, Multidisciplinary SC Engineering; Materials Science GA BJH84 UT WOS:000265961100211 ER PT S AU Neudeck, PG Spry, DJ Chen, LY Chang, CW Beheim, GM Okojie, RS Evans, LJ Meredith, RD Ferrier, TL Krasowski, MJ Prokop, NF AF Neudeck, Philip G. Spry, David J. Chen, Liang-Yu Chang, Carl W. Beheim, Glenn M. Okojie, Robert S. Evans, Laura J. Meredith, Roger D. Ferrier, Terry L. Krasowski, Michael J. Prokop, Norman F. BE PerezTomas, A Godignon, P Vellvehi, M Brosselard, P TI Prolonged 500 degrees C Operation of 6H-SiC JFET Integrated Circuitry SO SILICON CARBIDE AND RELATED MATERIALS 2008 SE Materials Science Forum LA English DT Proceedings Paper CT 7th European Conference on Silicon Carbide and Related Materials CY SEP 07-11, 2008 CL Barcelona, SPAIN SP Minist Educ & Cienc, ACCIO, Generalitat Catalunya, ACREO, Aixtron, Cree Inc, Dow Corning, D plus T Microelect, Ion Beam Serv, SiCED, SiCrystal AG DE 6H-SiC; JFET; high temperature; integrated circuit; amplifier; logic gate ID 500-DEGREES-C AB This paper updates the long-term 500 degrees C electrical testing results from 6H-SiC junction field effect transistors (JFETs) and small integrated circuits that were introduced at ICSCRM-2007. Two packaged JFETs have now been operated in excess of 7000 hours at 500 degrees C with less than 10% degradation in linear I-V characteristics. Several simple digital and analog demonstration integrated circuits Successfully operated for 2000-6500 hours at 500 degrees C before failure. C1 [Neudeck, Philip G.; Spry, David J.; Beheim, Glenn M.; Okojie, Robert S.; Evans, Laura J.; Meredith, Roger D.; Ferrier, Terry L.; Krasowski, Michael J.; Prokop, Norman F.] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. [Chen, Liang-Yu] NASA Glenn, OAI, Cleveland, OH 44135 USA. [Chang, Carl W.] ASRC Aerosp Corp, Cleveland, OH 44135 USA. RP Neudeck, PG (reprint author), NASA, Glenn Res Ctr, 21000 Brookpk Rd,MS 77-1, Cleveland, OH 44135 USA. EM neudeck@nasa.gov; david.j.spry@nasa.gov; liangyu.chen-1@nasa.gov RI Vellvehi, Miquel/J-8009-2014 OI Vellvehi, Miquel/0000-0002-0127-4690 NR 8 TC 12 Z9 12 U1 0 U2 0 PU TRANS TECH PUBLICATIONS LTD PI STAFA-ZURICH PA LAUBLSRUTISTR 24, CH-8717 STAFA-ZURICH, SWITZERLAND SN 0255-5476 J9 MATER SCI FORUM PY 2009 VL 615-617 BP 929 EP 932 PG 4 WC Engineering, Electrical & Electronic; Materials Science, Ceramics; Materials Science, Multidisciplinary SC Engineering; Materials Science GA BJH84 UT WOS:000265961100225 ER PT S AU Malaguti, G Angelini, L Raimondi, L Moretti, A Trifoglio, M AF Malaguti, G. Angelini, L. Raimondi, L. Moretti, A. Trifoglio, M. BE Ferrando, P Rodriguez, J TI Simbol-X Telescope Scientific Calibrations: Requirements and Plans SO SIMBOL-X: FOCUSING ON THE HARD X-RAY UNIVERSE SE AIP Conference Proceedings LA English DT Proceedings Paper CT 2nd International Simbol-X Symposium CY DEC 02-05, 2008 CL Paris, FRANCE SP CNES, ASI, CEA, CNRS, Univ Paris, GDR-PCHE, IN2P3, CESR DE Simbol-X; calibrations; end-to-end test AB The Simbol-X telescope characteristics and the mission scientific requirements impose a challenging calibration plan with a number of unprecedented issues. The 20 m focal length implies for the incoming X-ray beam a divergence comparable to the incidence angle of the mirror surface also for 100 m-long facilities. Moreover this is the first time that a direct focussing X-ray telescope will be calibrated on an energy band covering about three decades, and with a complex focal plane. These problems require a careful plan and organization of the measurements, together with an evaluation of the calibration needs in terms of both hardware and software. C1 [Malaguti, G.; Raimondi, L.; Trifoglio, M.] INAF IASF, Bologna, Italy. [Angelini, L.] NASA Goddard Space Flight Ctr, Greenbelt, MD USA. [Moretti, A.] INAF OABrera, Milan, Italy. RP Malaguti, G (reprint author), INAF IASF, Bologna, Italy. RI Trifoglio, Massimo/F-5302-2015 OI Malaguti, Giuseppe/0000-0001-9872-3378; moretti, alberto/0000-0002-9770-0315; Trifoglio, Massimo/0000-0002-2505-3630 NR 3 TC 0 Z9 0 U1 0 U2 0 PU AMER INST PHYSICS PI MELVILLE PA 2 HUNTINGTON QUADRANGLE, STE 1NO1, MELVILLE, NY 11747-4501 USA SN 0094-243X BN 978-0-7354-0662-9 J9 AIP CONF PROC PY 2009 VL 1126 BP 85 EP + PG 2 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BJM09 UT WOS:000266785900021 ER PT S AU Gehrels, N Cannizzo, JK AF Gehrels, Neil Cannizzo, John K. BE Ferrando, P Rodriguez, J TI The Hard X-ray Sky: Recent Observational Progress SO SIMBOL-X: FOCUSING ON THE HARD X-RAY UNIVERSE SE AIP Conference Proceedings LA English DT Proceedings Paper CT 2nd International Simbol-X Symposium CY DEC 02-05, 2008 CL Paris, FRANCE SP CNES, ASI, CEA, CNRS, Univ Paris, GDR-PCHE, IN2P3, CESR DE X- and gamma-rays: telescopes and instrumentation, observations; Sky surveys; X-ray binaries; The Galaxy: center; disk; Galaxies: AGN; Seyfert ID GALACTIC-CENTER; MILKY-WAY; CATALOG AB The last fifty years have witnessed the birth, development, and maturation to full potential of hard X-ray astrophysics. The primary force driving the history of the field has been the development of space-based instrumentation optimized for getting the maximum science out of observations of high-energy photons from astrophysical sources. Hard X-ray telescopes are leading research in areas such as galactic diffuse emission, galactic transients, and active galactic nuclei. C1 [Gehrels, Neil] NASA, GSFC, ASD, Code 661, Greenbelt, MD 20071 USA. [Cannizzo, John K.] CRESST, UMBC, GSFC, ASD, Greenbelt, MD 20071 USA. RP Gehrels, N (reprint author), NASA, GSFC, ASD, Code 661, Greenbelt, MD 20071 USA. RI Gehrels, Neil/D-2971-2012 NR 10 TC 0 Z9 0 U1 0 U2 0 PU AMER INST PHYSICS PI MELVILLE PA 2 HUNTINGTON QUADRANGLE, STE 1NO1, MELVILLE, NY 11747-4501 USA SN 0094-243X BN 978-0-7354-0662-9 J9 AIP CONF PROC PY 2009 VL 1126 BP 99 EP + PG 2 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BJM09 UT WOS:000266785900025 ER PT S AU Beckmann, V Courvoisier, TJL Gehrels, N Lubinski, P Malzac, J Petrucci, PO Shrader, CR Soldi, S AF Beckmann, V. Courvoisier, T. J. -L. Gehrels, N. Lubinski, P. Malzac, J. Petrucci, P. O. Shrader, C. R. Soldi, S. BE Ferrando, P Rodriguez, J TI Compton Reflection in AGN with Simbol-X SO SIMBOL-X: FOCUSING ON THE HARD X-RAY UNIVERSE SE AIP Conference Proceedings LA English DT Proceedings Paper CT 2nd International Simbol-X Symposium CY DEC 02-05, 2008 CL Paris, FRANCE SP CNES, ASI, CEA, CNRS, Univ Paris, GDR-PCHE, IN2P3, CESR DE Galaxies: active; Galaxies: Seyfert; X-rays: galaxies ID ACTIVE GALACTIC NUCLEI; LUMINOSITY FUNCTION; SPECTRUM; GALAXIES; ORIGIN AB AGN exhibit complex hard X-ray spectra. Our current understanding is that the emission is dominated by inverse Compton processes which take place in the corona above the accretion disk, and that absorption and reflection in a distant absorber play a major role. These processes can be directly observed through the shape of the continuum, the Compton reflection hump around 30 keV, and the iron fluorescence line at 6.4 keV. We demonstrate the capabilities of Simbol-X to constrain complex models for cases like MCG-05-23-016, NGC 4151, NGC 2110, and NGC 4051 in short (10 ksec) observations. We compare the simulations with recent observations on these sources by INTEGRAL, Swift and Suzaku. Constraining reflection models for AGN with Simbol-X will help us to get a clear view of the processes and geometry near to the central engine in AGN, and will give insight to which sources are responsible for the Cosmic X-ray background at energies > 20keV. C1 [Beckmann, V.; Courvoisier, T. J. -L.; Soldi, S.] ISDC Data Ctr Astrophys, Ch Ecogia 16, CH-1290 Versoix, Switzerland. [Gehrels, N.; Shrader, C. R.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Lubinski, P.] Centrum Astronomiczne, PL-00716 Warsaw, Poland. [Malzac, J.] CNRS, CESR, F-31028 Toulouse, France. [Petrucci, P. O.] CNRS, Lab Astrophys Grenoble, F-38041 Grenoble, France. RP Beckmann, V (reprint author), ISDC Data Ctr Astrophys, Ch Ecogia 16, CH-1290 Versoix, Switzerland. RI Gehrels, Neil/D-2971-2012 NR 18 TC 1 Z9 1 U1 0 U2 0 PU AMER INST PHYSICS PI MELVILLE PA 2 HUNTINGTON QUADRANGLE, STE 1NO1, MELVILLE, NY 11747-4501 USA SN 0094-243X BN 978-0-7354-0662-9 J9 AIP CONF PROC PY 2009 VL 1126 BP 141 EP + PG 2 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BJM09 UT WOS:000266785900034 ER PT S AU Raimondi, L Malaguti, G Angelini, L Cappi, M Grandi, P Palumbo, GGC Puccetti, S AF Raimondi, L. Malaguti, G. Angelini, L. Cappi, M. Grandi, P. Palumbo, G. G. C. Puccetti, S. BE Ferrando, P Rodriguez, J TI The Galactic Center View with Simbol-X SO SIMBOL-X: FOCUSING ON THE HARD X-RAY UNIVERSE SE AIP Conference Proceedings LA English DT Proceedings Paper CT 2nd International Simbol-X Symposium CY DEC 02-05, 2008 CL Paris, FRANCE SP CNES, ASI, CEA, CNRS, Univ Paris, GDR-PCHE, IN2P3, CESR DE Simbol-X; simulations; Galactic Centre; diffuse emission AB The nature of the hard X-ray emission above 3 keV of the Galactic Centre (GC) is still source of controversy. Recent observations with Chandra are consistent with either a population of discrete sources or with a diffuse non thermal emission or, most likely, a combination of the two. The Simbol-X mission will be equipped with a grazing incident telescope imaging up to similar to 80 keV, providing an improvement of three orders of magnitude in sensitivity and angular resolution compared with the instruments that have operated so far above 10 keV. This capability will enable to directly disentangle between the discrete source versus the diffuse emission scenarios. This is demonstrated by the Simbol-X simulations of the GC shown here, where the input model includes a list of both diffuse and point sources (both resolved and unresolved) using the input spectrum observed with presently operating X-ray telescopes. C1 [Raimondi, L.; Malaguti, G.; Cappi, M.; Grandi, P.] IASF Bologna, INAF, Bologna, Italy. [Angelini, L.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Palumbo, G. G. C.] Univ Bologna, I-40126 Bologna, Italy. [Puccetti, S.] ASI Sci Data Ctr, Rome, Italy. RP Raimondi, L (reprint author), IASF Bologna, INAF, Bologna, Italy. RI Cappi, Massimo/F-4813-2015; OI Cappi, Massimo/0000-0001-6966-8920; Malaguti, Giuseppe/0000-0001-9872-3378; Grandi, Paola/0000-0003-1848-6013; Puccetti, Simonetta/0000-0002-2734-7835 FU Italian Space Agency; ASI INAF [ASI- 1/088/06/0] FX We thank the Italian Space Agency for support under contract ASI INAF ASI- 1/088/06/0. NR 6 TC 0 Z9 0 U1 0 U2 0 PU AMER INST PHYSICS PI MELVILLE PA 2 HUNTINGTON QUADRANGLE, STE 1NO1, MELVILLE, NY 11747-4501 USA SN 0094-243X BN 978-0-7354-0662-9 J9 AIP CONF PROC PY 2009 VL 1126 BP 153 EP + PG 2 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BJM09 UT WOS:000266785900037 ER PT S AU Migliori, G Grandi, P Angelini, L Raimondi, L Torresi, E Palumbo, GGC AF Migliori, G. Grandi, P. Angelini, L. Raimondi, L. Torresi, E. Palumbo, G. G. C. BE Ferrando, P Rodriguez, J TI Powerful Radio Galaxies with Simbol-X: Lobes and Hot Spots SO SIMBOL-X: FOCUSING ON THE HARD X-RAY UNIVERSE SE AIP Conference Proceedings LA English DT Proceedings Paper CT 2nd International Simbol-X Symposium CY DEC 02-05, 2008 CL Paris, FRANCE SP CNES, ASI, CEA, CNRS, Univ Paris, GDR-PCHE, IN2P3, CESR DE galaxies: active; galaxies: individual (Pictor A); radiation mechanisms: non thermal ID RAY-EMISSION; PICTOR-A AB We present here the first Simbol-X simulations of the extended components, lobes and hot spots, of the radio galaxies. We use the paradigmatic case of Pictor A to test the capabilities of Simbol-X in this field of studies. Simulations demonstrate that Simbol-X will be able not only to perform spatially resolved studies on the lobes of radio galaxies below 10 keV but also to observe, for the first time, hard X-ray emission from the hot spots. These extremely promising results show the considerable potentiality of Simbol-X in studying interaction phenomena between relativistic plasma and surrounding environment. C1 [Migliori, G.] ISAS, SISSA, Via Beirut 2-4, I-34014 Trieste, Italy. [Grandi, P.; Raimondi, L.; Torresi, E.] INAF, IASF Bologna, I-34014 Trieste, Italy. [Angelini, L.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Palumbo, G. G. C.] Univ Bologna, Dipartimento Astronomia, I-40126 Bologna, Italy. RP Migliori, G (reprint author), ISAS, SISSA, Via Beirut 2-4, I-34014 Trieste, Italy. OI Grandi, Paola/0000-0003-1848-6013; TORRESI, ELEONORA/0000-0002-5201-010X FU Asi Science Data Center FX The authors thank S. Puccetti (Asi Science Data Center) for the support provided in the simulations. NR 6 TC 0 Z9 0 U1 0 U2 0 PU AMER INST PHYSICS PI MELVILLE PA 2 HUNTINGTON QUADRANGLE, STE 1NO1, MELVILLE, NY 11747-4501 USA SN 0094-243X BN 978-0-7354-0662-9 J9 AIP CONF PROC PY 2009 VL 1126 BP 156 EP + PG 2 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BJM09 UT WOS:000266785900038 ER PT S AU de Martino, D Anzolin, G Bonnet-Bidaud, JM Falanga, M Matt, G Mouchet, M Mukai, K Masetti, N AF de Martino, D. Anzolin, G. Bonnet-Bidaud, J. -M. Falanga, M. Matt, G. Mouchet, M. Mukai, K. Masetti, N. BE Ferrando, P Rodriguez, J TI Exploring the Hard and Soft X-ray Emission of Magnetic Cataclysmic Variables SO SIMBOL-X: FOCUSING ON THE HARD X-RAY UNIVERSE SE AIP Conference Proceedings LA English DT Proceedings Paper CT 2nd International Simbol-X Symposium CY DEC 02-05, 2008 CL Paris, FRANCE SP CNES, ASI, CEA, CNRS, Univ Paris, GDR-PCHE, IN2P3, CESR DE X-rays; Accretion and Accretion Disks; Cataclysmic Binaries ID INTERMEDIATE POLAR; WHITE-DWARF; IDENTIFICATION AB A non-negligible fraction of galactic hard (>20keV) X-ray sources were identified as CVs of the magnetic Intermediate Polar type in INTEGRAL, SWIFT and RXTE surveys, that suggests a still hidden but potentially important population of faint hard X-ray sources. Simbol-X has the unique potential to simultaneously characterize their variable and complex soft and hard X-ray emission thus allowing to understand their putative role in galactic populations of X-ray sources. C1 [de Martino, D.; Anzolin, G.] INAF Osservatorio Astron Capodimonte, Via Moiariello 16, I-80131 Naples, Italy. [Bonnet-Bidaud, J. -M.; Falanga, M.] Saclay Gif Sur Yvette, Serv Astrophys, Gif Sur Yvette, France. [Matt, G.] Univ Rome Tre, Dipartmento Fis, Rome, Italy. [Mouchet, M.] Univ Paris 07, Lab APC, Paris, France. [Mukai, K.] NASA, GSFC, CRESST & X Ray Astrophys Lab, Greenbelt, MD 20771 USA. [Masetti, N.] INAF IASF Bologna, Bologna, Italy. RP de Martino, D (reprint author), INAF Osservatorio Astron Capodimonte, Via Moiariello 16, I-80131 Naples, Italy. OI de Martino, Domitilla/0000-0002-5069-4202 FU ASI [1/023/05/06, 1/088/06/0]; INAF [PRIN-INAF/2007/17] FX We acknowledge financial support from ASI under contracts 1/023/05/06 and 1/088/06/0 and INAF under contract PRIN-INAF/2007/17. NR 25 TC 0 Z9 0 U1 0 U2 0 PU AMER INST PHYSICS PI MELVILLE PA 2 HUNTINGTON QUADRANGLE, STE 1NO1, MELVILLE, NY 11747-4501 USA SN 0094-243X BN 978-0-7354-0662-9 J9 AIP CONF PROC PY 2009 VL 1126 BP 210 EP + PG 2 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BJM09 UT WOS:000266785900052 ER PT S AU Paizis, A Farinelli, R Titarchuk, L Frontera, F Cocchi, M Ferrigno, C AF Paizis, A. Farinelli, R. Titarchuk, L. Frontera, F. Cocchi, M. Ferrigno, C. BE Ferrando, P Rodriguez, J TI A New Comptonization Model for Weakly Magnetized Accreting NS LMXBs SO SIMBOL-X: FOCUSING ON THE HARD X-RAY UNIVERSE SE AIP Conference Proceedings LA English DT Proceedings Paper CT 2nd International Simbol-X Symposium CY DEC 02-05, 2008 CL Paris, FRANCE SP CNES, ASI, CEA, CNRS, Univ Paris, GDR-PCHE, IN2P3, CESR DE X-ray binaries; Accretion and accretion disks; Neutron stars ID X-RAY BINARIES; NEUTRON-STAR; FLOW AB We have developed a new Comptonization model to propose, for the first time, a self consistent physical interpretation of the complex spectral evolution seen in NS LMXBs. The model and its application to LMXBs are presented and compared to the Simbol-X expected capabilities. C1 [Paizis, A.] INAF IASF Milano, Milan, Italy. [Farinelli, R.; Titarchuk, L.; Frontera, F.] Univ Ferrara, Dept Fis, I-44100 Ferrara, Italy. [Titarchuk, L.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Cocchi, M.] INAF IASF, Rome, Italy. [Ferrigno, C.] INTEGRAL Sci Data Ctr, Geneva, Switzerland. RP Paizis, A (reprint author), INAF IASF Milano, Milan, Italy. OI Paizis, Adamantia/0000-0001-5067-0377 FU ASI [1/008/07/0]; "Bulk motion Comptonization models in XRBs: from phenomenology to physics", Italian [PRIN-INAF] FX AP acknowledges ASI financial and programmatic support (contract1/008/07/0). This work has been partially supported by the Italian PRIN-INAF 2007 grant, "Bulk motion Comptonization models in XRBs: from phenomenology to physics", PI M. Cocchi. NR 11 TC 0 Z9 0 U1 0 U2 0 PU AMER INST PHYSICS PI MELVILLE PA 2 HUNTINGTON QUADRANGLE, STE 1NO1, MELVILLE, NY 11747-4501 USA SN 0094-243X BN 978-0-7354-0662-9 J9 AIP CONF PROC PY 2009 VL 1126 BP 316 EP + PG 2 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BJM09 UT WOS:000266785900076 ER PT B AU Clancey, WJ AF Clancey, William J. BA Turkle, S BF Turkle, S TI BECOMING A ROVER SO SIMULATION AND ITS DISCONTENTS SE Simplicity-Design Technology Business Life LA English DT Article; Book Chapter C1 [Clancey, William J.] NASA, Ames Res Ctr, Washington, DC 20546 USA. RP Clancey, WJ (reprint author), NASA, Ames Res Ctr, Washington, DC 20546 USA. NR 6 TC 2 Z9 2 U1 0 U2 0 PU M I T PRESS PI CAMBRIDGE PA FIVE CAMBRIDGE CENTER, CAMBRIDGE, MA 02142 USA BN 978-0-262-01270-6 J9 SIMPLICITY-DES TECHN PY 2009 BP 107 EP + PG 25 WC Computer Science, Artificial Intelligence; Computer Science, Theory & Methods; Operations Research & Management Science SC Computer Science; Operations Research & Management Science GA BOZ16 UT WOS:000278096100007 ER PT B AU Matsko, AB Maleki, L AF Matsko, Andrey B. Maleki, Lute BE Khurgin, JB Tucker, RS TI Resonator-Mediated Slow Light: Novel Structures, Applications and Tradeoffs SO SLOW LIGHT: SCIENCE AND APPLICATIONS SE Optical Science and Engineering-CRC LA English DT Article; Book Chapter ID OPTOELECTRONIC MICROWAVE-OSCILLATOR; ELECTROMAGNETICALLY INDUCED TRANSPARENCY; OPTICAL WAVE-GUIDES; GROUP-VELOCITY; ATOMIC GAS; DELAY; FILTERS; TRANSMISSION; PROPAGATION; SYSTEMS C1 [Matsko, Andrey B.; Maleki, Lute] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. RP Matsko, AB (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. NR 62 TC 0 Z9 0 U1 0 U2 1 PU CRC PRESS-TAYLOR & FRANCIS GROUP PI BOCA RATON PA 6000 BROKEN SOUND PARKWAY NW, STE 300, BOCA RATON, FL 33487-2742 USA BN 978-1-4200-6151-2 J9 OPT SCI ENG-CRC PY 2009 VL 140 BP 101 EP 117 PG 17 WC Engineering, Electrical & Electronic; Optics; Physics, Applied; Physics, Particles & Fields SC Engineering; Optics; Physics GA BJU13 UT WOS:000267161300006 ER PT B AU Boroson, DM Scozzafava, JJ Murphy, DV Robinson, BS Shaw, H AF Boroson, D. M. Scozzafava, J. J. Murphy, D. V. Robinson, B. S. Shaw, H. GP IEEE COMPUTER SOC TI The Lunar Laser Communications Demonstration (LLCD) SO SMC-IT 2009: THIRD IEEE INTERNATIONAL CONFERENCE ON SPACE MISSION CHALLENGES FOR INFORMATION TECHNOLOGY, PROCEEDINGS LA English DT Proceedings Paper CT 3rd IEEE International Conference on Space Mission Challenges for Information Technology CY JUL 19-23, 2009 CL Pasadena, CA SP IEEE AB NASA is presently overseeing a project to create the world's first free-space laser communications system that can be operated over a range ten times larger than the near-earth ranges that have been demonstrated to date. To be flown on the Lunar Atmosphere and Dust Environment Explorer (LADEE), which is planned for launch by NASA in 2012, it will demonstrate high-rate laser communications from Lunar orbit to a transportable ground terminal on the Earth. To support up to 622 Mbps over the approximately 400 thousand kilometer link, the system will make use of a high peak-power doped-fiber transmitter, a hybrid pointing and tracking system, high efficiency modulation and coding techniques, superconducting photon-counting detectors, and a scalable optical collector architecture. It also will support up to 20 Mbps on the optical uplink, plus a highly accurate continuous two-way time-of-flight measurement capability with the potential to perform ranging with sub-centimeter accuracy to the moving spacecraft. The project is being undertaken by MIT Lincoln Laboratory (MIT/LL) and the NASA Goddard Space Flight Center (GSFC.) C1 [Boroson, D. M.; Scozzafava, J. J.; Murphy, D. V.; Robinson, B. S.] MIT, Lincoln Lab, 244 Wood St, Lexington, MA 02173 USA. [Shaw, H.] NASA, Goddard Space Flight cTR, Greenbelt, MD USA. RP Boroson, DM (reprint author), MIT, Lincoln Lab, 244 Wood St, Lexington, MA 02173 USA. EM boroson@ll.mit.edu NR 10 TC 12 Z9 13 U1 2 U2 12 PU IEEE COMPUTER SOC PI LOS ALAMITOS PA 10662 LOS VAQUEROS CIRCLE, PO BOX 3014, LOS ALAMITOS, CA 90720-1264 USA BN 978-0-7695-3637-8 PY 2009 BP 23 EP + DI 10.1109/SMC-IT.2009.57 PG 3 WC Engineering, Aerospace SC Engineering GA BMO51 UT WOS:000273122700003 ER PT B AU Wang, SY Torgerson, JL Schoolcraft, J Brenman, Y AF Wang, Shin-Ywan (Cindy) Torgerson, J. Leigh Schoolcraft, Joshua Brenman, Yan GP IEEE COMPUTER SOC TI The Deep Impact Network Experiment Operations Center Monitor and Control System SO SMC-IT 2009: THIRD IEEE INTERNATIONAL CONFERENCE ON SPACE MISSION CHALLENGES FOR INFORMATION TECHNOLOGY, PROCEEDINGS LA English DT Proceedings Paper CT 3rd IEEE International Conference on Space Mission Challenges for Information Technology CY JUL 19-23, 2009 CL Pasadena, CA SP IEEE DE Deep Impack Network (DINET); Delay/Disruption Tolerant Network (DTN); Interplanetary Overlay Network (ION); Bundle Protocol (BP); Experiment Operations Center (EOC); Asynchronous Message System (AMS); Protocol Technology Lab (PTL) AB The Interplanetary Overlay Network (ION) software at JPL is an implementation of Delay/Disruption Tolerant Networking (DTN) which has been proposed as an interplanetary protocol to support space communication. The JPL Deep Impact Network (DINET) is a technology development experiment intended to increase the technical readiness of the JPL implemented ION suite. The DINET Experiment Operations Center (EOC) developed by JPL's Protocol Technology Lab (PTL) was critical in accomplishing the experiment. EOC, containing all end nodes of simulated spaces and one administrative node, exercised publish and subscribe functions for payload data among all end nodes to verify the effectiveness of data exchange over ION protocol stacks. A Monitor and Control System was created and installed on the administrative node as a multi-tiered internet-based Web application to support the Deep Impact Network Experiment by allowing monitoring and analysis of the data delivery and statistics from ION. This Monitor and Control System includes the capability of receiving protocol status messages, classifying and storing status messages into a database from the ION simulation network, and providing web interfaces for viewing the live results in addition to interactive database queries. C1 [Wang, Shin-Ywan (Cindy); Torgerson, J. Leigh; Schoolcraft, Joshua; Brenman, Yan] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Wang, SY (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM Shin-Ywan.Wang@jpl.nasa.gov; Jordan.L.Torgerson@jpl.nasa.gov; Joshua.Schoolcraft@jpl.nasa.gov; Bremann.Yan@jpl.nasa.gov NR 5 TC 2 Z9 2 U1 0 U2 0 PU IEEE COMPUTER SOC PI LOS ALAMITOS PA 10662 LOS VAQUEROS CIRCLE, PO BOX 3014, LOS ALAMITOS, CA 90720-1264 USA BN 978-0-7695-3637-8 PY 2009 BP 34 EP 40 DI 10.1109/SMC-IT.2009.13 PG 7 WC Engineering, Aerospace SC Engineering GA BMO51 UT WOS:000273122700005 ER PT B AU Wang, YF Schrock, M Baldwin, J Rangel, G Borden, C AF Wang, Yeou-Fang Schrock, Mitchell Baldwin, John Rangel, Gabriel Borden, Chester GP IEEE COMPUTER SOC TI Web 2.0 for Ground Resource Allocation SO SMC-IT 2009: THIRD IEEE INTERNATIONAL CONFERENCE ON SPACE MISSION CHALLENGES FOR INFORMATION TECHNOLOGY, PROCEEDINGS LA English DT Proceedings Paper CT 3rd IEEE International Conference on Space Mission Challenges for Information Technology CY JUL 19-23, 2009 CL Pasadena, CA SP IEEE DE resource management; planning; Internet AB A set of analysis tools has been created in a community-based team environment to support NASA ground resource allocation and planning. This new tool, called GRAPE (Ground Resource Allocation and Planning Environment), combines analysis, monitoring, and search capabilities into an existing community environment where wikis, blogs, document libraries, calendars, discussion forums, lists, progress management, and email repositories are available in a web site which assists users with their communication, operation, analysis, and collaboration needs. C1 [Wang, Yeou-Fang; Schrock, Mitchell; Baldwin, John; Rangel, Gabriel; Borden, Chester] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. RP Wang, YF (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. EM Yeou-Fang.Wang@jpl.nasa.gov NR 1 TC 0 Z9 0 U1 0 U2 0 PU IEEE COMPUTER SOC PI LOS ALAMITOS PA 10662 LOS VAQUEROS CIRCLE, PO BOX 3014, LOS ALAMITOS, CA 90720-1264 USA BN 978-0-7695-3637-8 PY 2009 BP 51 EP 57 DI 10.1109/SMC-IT.2009.15 PG 7 WC Engineering, Aerospace SC Engineering GA BMO51 UT WOS:000273122700007 ER PT B AU Policella, N Oliveira, H Siili, T AF Policella, Nicola Oliveira, Henrique Siili, Tero GP IEEE COMPUTER SOC TI SKEYP: AI applied to SOHO Keyhole Operations SO SMC-IT 2009: THIRD IEEE INTERNATIONAL CONFERENCE ON SPACE MISSION CHALLENGES FOR INFORMATION TECHNOLOGY, PROCEEDINGS LA English DT Proceedings Paper CT 3rd IEEE International Conference on Space Mission Challenges for Information Technology CY JUL 19-23, 2009 CL Pasadena, CA SP IEEE AB The Solar and Heliospheric Observatory's (SOHO) mission operations team has - due to a spacecraft malfunction - had to deal with the Keyhole Periods problem since 2003. This combinatorial problem arises from the conflict between limited telemetry downlink capabilities during keyhole periods and the need to maximize the return of science data while respecting other constraints, such as limited on-board storage capacity. Until recently, this problem has been addressed by manually generating data production and downlink plans. This work presents the SOHO Keyhole Planner (SKEYP), a software tool designed to improve on the manual workflow for plan generation by shortening the time needed and reduce significance of the learning curve associated with this process. C1 [Policella, Nicola; Oliveira, Henrique] European Space Agcy, European Space Operat Ctr, Darmstadt, Germany. [Siili, Tero] Goddard Space Flight Ctr, European Space Agcy, SOHO Team, Greenbelt, MD USA. RP Policella, N (reprint author), European Space Agcy, European Space Operat Ctr, Darmstadt, Germany. EM nicola.policella@esa.int; henrique.oliveira@esa.int; tero.siili@esa.int NR 7 TC 0 Z9 0 U1 0 U2 0 PU IEEE COMPUTER SOC PI LOS ALAMITOS PA 10662 LOS VAQUEROS CIRCLE, PO BOX 3014, LOS ALAMITOS, CA 90720-1264 USA BN 978-0-7695-3637-8 PY 2009 BP 58 EP + DI 10.1109/SMC-IT.2009.16 PG 2 WC Engineering, Aerospace SC Engineering GA BMO51 UT WOS:000273122700008 ER PT B AU Morris, R Dungan, J Votava, P AF Morris, Robert Dungan, Jennifer Votava, Petr GP IEEE COMPUTER SOC TI A Workflow Model for Earth Observation Sensor Webs SO SMC-IT 2009: THIRD IEEE INTERNATIONAL CONFERENCE ON SPACE MISSION CHALLENGES FOR INFORMATION TECHNOLOGY, PROCEEDINGS LA English DT Proceedings Paper CT 3rd IEEE International Conference on Space Mission Challenges for Information Technology CY JUL 19-23, 2009 CL Pasadena, CA SP IEEE DE Sensor Webs; Workflow Management System AB An Earth science sensor web consists of a distributed collection of sensors, Earth science models, human scientists and information technologists, and data archives. The scientific use of the sensor web consists broadly of seeking to improve the understanding of natural processes occurring on the Earth's surface or in the atmosphere. Sensor measurements serve to quantify aspects of these processes that allow Earth science models to make predictions of scientific and social value. The management problem for sensor webs considered here is the problem of reconfiguring the sensor web in order to answer new science questions. The notion of reconfiguration is used broadly here to describe a set of actions for retargeting sensors, querying databases for image data, or executing functions foe analyzing acquired data. This paper describes a workflow model and architecture for a workflow management system for reconfiguring sensor webs. C1 [Morris, Robert; Dungan, Jennifer; Votava, Petr] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Morris, R (reprint author), NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. EM robert.a.morris@nasa.gov; jennifer.l.dungan@nasa.gov; petr.votava@nasa.gov OI /0000-0002-4863-1616 NR 8 TC 3 Z9 3 U1 0 U2 0 PU IEEE COMPUTER SOC PI LOS ALAMITOS PA 10662 LOS VAQUEROS CIRCLE, PO BOX 3014, LOS ALAMITOS, CA 90720-1264 USA BN 978-0-7695-3637-8 PY 2009 BP 69 EP 76 DI 10.1109/SMC-IT.2009.60 PG 8 WC Engineering, Aerospace SC Engineering GA BMO51 UT WOS:000273122700009 ER PT B AU Pasareanu, CS Schumann, J Mehlitz, P Lowry, M Karsai, G Nine, H Neema, S AF Pasareanu, Corina S. Schumann, Johann Mehlitz, Peter Lowry, Mike Karsai, Gabor Nine, Harmon Neema, Sandeep GP IEEE COMPUTER SOC TI Model Based Analysis and Test Generation for Flight Software SO SMC-IT 2009: THIRD IEEE INTERNATIONAL CONFERENCE ON SPACE MISSION CHALLENGES FOR INFORMATION TECHNOLOGY, PROCEEDINGS LA English DT Proceedings Paper CT 3rd IEEE International Conference on Space Mission Challenges for Information Technology CY JUL 19-23, 2009 CL Pasadena, CA SP IEEE ID SEMANTICS AB We describe a framework for model-based analysis and test case generation in the context of a heterogeneous model-based development paradigm that uses and combines MathWorks and UML 2.0 models and the associated code generation tools. This paradigm poses novel challenges to analysis and test case generation that, to the best of our knowledge, have not been addressed before. The framework is based on a common intermediate representation for different modeling formalisms and leverages and extends model checking and symbolic execution tools for model analysis and test case generation, respectively. We discuss the application of our framework to software models for a NASA flight mission. C1 [Pasareanu, Corina S.; Schumann, Johann; Mehlitz, Peter; Lowry, Mike] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Karsai, Gabor; Nine, Harmon; Neema, Sandeep] Vanderbilt Univ, ISIS, Nashville, TN 37235 USA. RP Pasareanu, CS (reprint author), NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. EM CORINASPASAREANU@nasa.gov; JOHANNSCHUMANN@nasa.gov; PETERMEHLITZ@nasa.gov; MIKELOWRY@nasa.gov; gabor@isis.vanderbilt.edu; hnine@isis.vanderbilt.edu; sandeep@isis.vanderbilt.edu NR 15 TC 5 Z9 5 U1 0 U2 0 PU IEEE COMPUTER SOC PI LOS ALAMITOS PA 10662 LOS VAQUEROS CIRCLE, PO BOX 3014, LOS ALAMITOS, CA 90720-1264 USA BN 978-0-7695-3637-8 PY 2009 BP 83 EP + DI 10.1109/SMC-IT.2009.18 PG 3 WC Engineering, Aerospace SC Engineering GA BMO51 UT WOS:000273122700011 ER PT B AU Barry, M Horvath, G AF Barry, Matthew Horvath, Gregory GP IEEE COMPUTER SOC TI Prototype Implementation of a Goal-Based Software Health Management Service SO SMC-IT 2009: THIRD IEEE INTERNATIONAL CONFERENCE ON SPACE MISSION CHALLENGES FOR INFORMATION TECHNOLOGY, PROCEEDINGS LA English DT Proceedings Paper CT 3rd IEEE International Conference on Space Mission Challenges for Information Technology CY JUL 19-23, 2009 CL Pasadena, CA SP IEEE AB The FAILSAFE project is developing concepts and prototype implementations for software health management in mission-critical real-time embedded systems. The project unites features of the industry standard ARINC 653 Avionics Application Software Standard Interface and JPL's Mission Data System (MDS) technology. The ARINC 653 standard establishes requirements for the services provided by partitioned real-time operating systems. The MDS technology provides a state analysis method, canonical architecture, and software framework that facilitates the design and implementation of software-intensive complex systems. We use the MDS technology to provide the health management function for an ARINC 653 application implementation. In particular, we focus on showing how this combination enables reasoning about and recovering from application software problems. Our prototype application software mimics the Space Shuttle orbiter's abort control sequencer software task, which provides safety-related functions to manage vehicle performance during launch aborts. We turned this task into a goal-based function that, when working in concert with the software health manager, aims to work around software and hardware problems in order to maximize abort performance results. In order to make it a compelling demonstration for current aerospace initiatives, we additionally imposed on our prototype a number of requirements derived from NASA's Constellation Program. Lastly, the ARINC 653 standard imposes a number of requirements on the system integrator for developing the requisite error handier process. Under ARINC 653, the health monitoring (HM) service is invoked by an application calling the application error service or by the operating system or hardware detecting a fault. It is these HM and error process details that we implement with the MDS technology, showing how a state-analytic approach is appropriate for identifying fault determination details, and showing how the framework supports acting upon state estimation and control features in order to achieve safety-related goals. We describe herein the requirements, design, and implementation of our software health manager and the software under control. We provide details of the analysis and design for the Phase II prototype, and describe future directions for the remainder of Phase II and the new topics we plan to address in Phase III. C1 [Barry, Matthew] Kestrel Technol LLC, 4984 El Camino Real, Los Altos, CA 94022 USA. [Horvath, Gregory] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Barry, M (reprint author), Kestrel Technol LLC, 4984 El Camino Real, Los Altos, CA 94022 USA. EM mrbarry@kestreltechnology.com; gregory.a.horvath@jpl.nasa.gov FU NASA Small Business Technology Transfer (STTR) [NNA07AA24C] FX The Failsafe project is sponsored by a NASA Small Business Technology Transfer (STTR) Phase II award under contract NNA07AA24C. NR 5 TC 2 Z9 2 U1 0 U2 2 PU IEEE COMPUTER SOC PI LOS ALAMITOS PA 10662 LOS VAQUEROS CIRCLE, PO BOX 3014, LOS ALAMITOS, CA 90720-1264 USA BN 978-0-7695-3637-8 PY 2009 BP 117 EP + DI 10.1109/SMC-IT.2009.21 PG 2 WC Engineering, Aerospace SC Engineering GA BMO51 UT WOS:000273122700015 ER PT B AU Granat, R Wagstaff, KL Bornstein, B Tang, BY Turmon, M AF Granat, Robert Wagstaff, Kiri L. Bornstein, Benjamin Tang, Benyang Turmon, Michael GP IEEE COMPUTER SOC TI Simulating and Detecting Radiation-Induced Errors for Onboard Machine Learning SO SMC-IT 2009: THIRD IEEE INTERNATIONAL CONFERENCE ON SPACE MISSION CHALLENGES FOR INFORMATION TECHNOLOGY, PROCEEDINGS LA English DT Proceedings Paper CT 3rd IEEE International Conference on Space Mission Challenges for Information Technology CY JUL 19-23, 2009 CL Pasadena, CA SP IEEE ID ALGORITHMIC FAULT TOLERANCE; NETWORKS AB Spacecraft processors and memory are subjected to high radiation doses and therefore employ radiation-hardened components. However, these components are orders of magnitude more expensive than typical desktop components, and they lag years behind in terms of speed and size. We have integrated algorithm-based fault tolerance (ABFT) methods into onboard data analysis algorithms to detect radiation-induced errors, which ultimately may permit the use of spacecraft memory that need not be fully hardened, reducing cost and increasing capability at the same time. We have also developed a lightweight software radiation simulator, BITFLIPS, that permits evaluation of error detection strategies in a controlled fashion, including the specification of the radiation rate and selective exposure of individual data structures. Using BITFLIPS, we evaluated our error detection methods when using a support vector machine to analyze data collected by the Mars Odyssey spacecraft. We observed good performance from both an existing ABFT method for matrix multiplication and a novel ABFT method for exponentiation. These techniques bring us a step closer to "rad-hard" machine learning algorithms. C1 [Granat, Robert; Wagstaff, Kiri L.; Bornstein, Benjamin; Tang, Benyang; Turmon, Michael] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Granat, R (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM robert.granat@jpl.nasa.gov; kiri.wagstaff@jpl.nasa.gov; benjamin.bornstein@jpl.nasa.gov; benyang.tang@jpl.nasa.gov; michael.turmon@jpl.nasa.gov OI Wagstaff, Kiri/0000-0003-4401-5506 NR 24 TC 0 Z9 0 U1 0 U2 0 PU IEEE COMPUTER SOC PI LOS ALAMITOS PA 10662 LOS VAQUEROS CIRCLE, PO BOX 3014, LOS ALAMITOS, CA 90720-1264 USA BN 978-0-7695-3637-8 PY 2009 BP 125 EP 131 DI 10.1109/SMC-IT.2009.22 PG 7 WC Engineering, Aerospace SC Engineering GA BMO51 UT WOS:000273122700016 ER PT B AU Zima, HP James, ML AF Zima, Hans P. James, Mark L. GP IEEE COMPUTER SOC TI Introspection-Based Verification and Validation SO SMC-IT 2009: THIRD IEEE INTERNATIONAL CONFERENCE ON SPACE MISSION CHALLENGES FOR INFORMATION TECHNOLOGY, PROCEEDINGS LA English DT Proceedings Paper CT 3rd IEEE International Conference on Space Mission Challenges for Information Technology CY JUL 19-23, 2009 CL Pasadena, CA SP IEEE AB Future missions of deep-space exploration will require an on-board computational capability that can support autonomy and enhanced science processing. The integration of emerging commodity multi-core technology into space-borne systems can provide the required performance; however, protecting such systems against faults has become a critical research issue. In this paper we present an approach to fault tolerance based On a newly developed introspection framework that supports runtime monitoring of program execution and feedback-oriented recovery. We discuss the relationship of this approach to traditional Verification. and Validation (V&V) and propose methods for the automatic generation of assertions front static and dynamic analysis. C1 [Zima, Hans P.; James, Mark L.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Zima, HP (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM zima@jpl.nasa.gov; mjames@jpl.nasa.gov NR 23 TC 0 Z9 0 U1 0 U2 0 PU IEEE COMPUTER SOC PI LOS ALAMITOS PA 10662 LOS VAQUEROS CIRCLE, PO BOX 3014, LOS ALAMITOS, CA 90720-1264 USA BN 978-0-7695-3637-8 PY 2009 BP 132 EP 139 DI 10.1109/SMC-IT.2009.23 PG 8 WC Engineering, Aerospace SC Engineering GA BMO51 UT WOS:000273122700017 ER PT B AU Smith, TB Chavez-Clemente, D AF Smith, Tristan B. Chavez-Clemente, Daniel GP IEEE COMPUTER SOC TI A Practical Comparison of Motion Planning Techniques for Robotic Legs in Environments with Obstacles SO SMC-IT 2009: THIRD IEEE INTERNATIONAL CONFERENCE ON SPACE MISSION CHALLENGES FOR INFORMATION TECHNOLOGY, PROCEEDINGS LA English DT Proceedings Paper CT 3rd IEEE International Conference on Space Mission Challenges for Information Technology CY JUL 19-23, 2009 CL Pasadena, CA SP IEEE AB ATHLETE is a large six-legged tele-operated robot. Each foot is a wheel; travel can be achieved by walking, rolling, or some combination of the two. Operators control ATHLETE by selecting parameterized commands front a command dictionary. While rolling can be done efficiently, any motion involving steps is cumbersome - each step can require multiple commands and take many minutes to complete. In this paper we consider four different algorithms that generate a sequence of commands to take a step. We consider a baseline heuristic, a randomized motion planning algorithm, and two variants of A* search. Results for a variety of terrains are presented, and we discuss the quantitative and qualitative tradeoffs between the approaches. C1 [Smith, Tristan B.] NASA, Ames Res Ctr, Mission Crit Technol Inc, Moffett Field, CA 94035 USA. [Chavez-Clemente, Daniel] Stanford Univ, Dept Aeronaut & Astronaut, Stanford, CA 94305 USA. RP Smith, TB (reprint author), NASA, Ames Res Ctr, Mission Crit Technol Inc, Moffett Field, CA 94035 USA. EM tristan.b.smith@nasa.gov; dchavez@stanford.edu NR 11 TC 0 Z9 1 U1 0 U2 0 PU IEEE COMPUTER SOC PI LOS ALAMITOS PA 10662 LOS VAQUEROS CIRCLE, PO BOX 3014, LOS ALAMITOS, CA 90720-1264 USA BN 978-0-7695-3637-8 PY 2009 BP 155 EP + DI 10.1109/SMC-IT.2009.26 PG 2 WC Engineering, Aerospace SC Engineering GA BMO51 UT WOS:000273122700020 ER PT B AU Mattmann, CA Freeborn, D Crichton, D Foster, B Hart, A Woollard, D Hardman, S Ramirez, P Kelly, S Chang, AY Miller, CE AF Mattmann, Chris A. Freeborn, Dana Crichton, Dan Foster, Brian Hart, Andrew Woollard, David Hardman, Sean Ramirez, Paul Kelly, Sean Chang, Albert Y. Miller, Charles E. GP IEEE COMPUTER SOC TI A Reusable Process Control System Framework for the Orbiting Carbon Observatory and NPP Sounder PEATE missions SO SMC-IT 2009: THIRD IEEE INTERNATIONAL CONFERENCE ON SPACE MISSION CHALLENGES FOR INFORMATION TECHNOLOGY, PROCEEDINGS LA English DT Proceedings Paper CT 3rd IEEE International Conference on Space Mission Challenges for Information Technology CY JUL 19-23, 2009 CL Pasadena, CA SP IEEE AB We describe a reusable architecture and implementation framework for managing science processing pipelines for mission ground data systems. Our system, dubbed "PCS", for Process Control System, improves upon an existing software component, the OODT Catalog and Archive (CAS), which has already supported the QuikSCAT SeaWinds and AMT earth. science missions. This paper focuses on PCS within the context of two current earth science missions: the Orbiting Carbon Observatory (OCO), and NPP Sounder PEATE projects. C1 [Mattmann, Chris A.; Freeborn, Dana; Crichton, Dan; Foster, Brian; Hart, Andrew; Woollard, David; Hardman, Sean; Ramirez, Paul; Kelly, Sean; Chang, Albert Y.; Miller, Charles E.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Mattmann, CA (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM mattmann@jpl.nasa.gov NR 12 TC 8 Z9 8 U1 0 U2 0 PU IEEE COMPUTER SOC PI LOS ALAMITOS PA 10662 LOS VAQUEROS CIRCLE, PO BOX 3014, LOS ALAMITOS, CA 90720-1264 USA BN 978-0-7695-3637-8 PY 2009 BP 165 EP 172 DI 10.1109/SMC-IT.2009.27 PG 8 WC Engineering, Aerospace SC Engineering GA BMO51 UT WOS:000273122700021 ER PT B AU Topousis, DE Means, EK Murphy, KS Yew, M AF Topousis, Daria E. Means, Erin K. Murphy, Keri S. Yew, Manson GP IEEE COMPUTER SOC TI Enhancing Collaboration Among NASA Engineers through a Knowledge Sharing System SO SMC-IT 2009: THIRD IEEE INTERNATIONAL CONFERENCE ON SPACE MISSION CHALLENGES FOR INFORMATION TECHNOLOGY, PROCEEDINGS LA English DT Proceedings Paper CT 3rd IEEE International Conference on Space Mission Challenges for Information Technology CY JUL 19-23, 2009 CL Pasadena, CA SP IEEE DE Communities of practice; information retrieval; knowledge based systems AB Because solar system exploration often involves highly complex missions, a strong infrastructure to support knowledge sharing among engineers is critical to facilitate problem solving and preserve solutions for future work. Any system developed to meet these needs must include the ability to rapidly disseminate content, connect users to the right information regardless of where it is stored, and connect people with the experts and they need. This paper describes the knowledge sharing solution called the NASA Engineering Network, which includes a faceted search, communities of practice, an expertise locator, and a centralized engineering portal. The paper includes details on how the components were developed and provides best practices that other aerospace organizations might use when implementing similar systems. C1 [Topousis, Daria E.; Means, Erin K.; Murphy, Keri S.; Yew, Manson] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Topousis, DE (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM daria.e.topousis@jpl.nasa.gov; erin.means@jpl.nasa.gov; keri.s.murphy@jpl.nasa.gov; manson.yew@jpl.nasa.gov NR 13 TC 0 Z9 0 U1 0 U2 6 PU IEEE COMPUTER SOC PI LOS ALAMITOS PA 10662 LOS VAQUEROS CIRCLE, PO BOX 3014, LOS ALAMITOS, CA 90720-1264 USA BN 978-0-7695-3637-8 PY 2009 BP 187 EP 192 DI 10.1109/SMC-IT.2009.29 PG 6 WC Engineering, Aerospace SC Engineering GA BMO51 UT WOS:000273122700024 ER PT B AU Troglio, G Benediktsson, JA Troglio, G Moser, G Serpico, SB Le Moigne, J AF Troglio, G. Benediktsson, J. A. Troglio, G. Moser, G. Serpico, S. B. Le Moigne, J. GP IEEE COMPUTER SOC TI Automatic Extraction of Planetary Image Features SO SMC-IT 2009: THIRD IEEE INTERNATIONAL CONFERENCE ON SPACE MISSION CHALLENGES FOR INFORMATION TECHNOLOGY, PROCEEDINGS LA English DT Proceedings Paper CT 3rd IEEE International Conference on Space Mission Challenges for Information Technology CY JUL 19-23, 2009 CL Pasadena, CA SP IEEE DE Crater detection; feature extraction; image segmentation; image registration ID CLASSIFICATION AB With the launch of several Lunar missions such as the Lunar Reconnaissance Orbiter (LRO) and Chandrayaan-1, a large amount of Lunar images will be acquired and will need to be analyzed. Although many automatic feature extraction methods have been proposed and utilized for Earth remote sensing images, these methods are not always applicable to Lunar data that often present low contrast and uneven illumination characteristics. In this paper, we propose a new method for the extraction of features from the Lunar surface, based on the combination of several image processing techniques, including a watershed segmentation and the generalized Hough Transform. The method has many applications, among which image registration, and can be generalized to other planetary images as well. C1 [Troglio, G.; Benediktsson, J. A.] Univ Iceland, Dept Elect & Comp Engn, Reykjavik, Iceland. [Troglio, G.; Moser, G.; Serpico, S. B.] Univ Genoa, Dept Biophys & Elect Engn, Genoa, Italy. [Le Moigne, J.] NASA, Goddard Space Flight Ctr, Software Engn Div, GSFC Code 580, Greenbelt, MD USA. RP Troglio, G (reprint author), Univ Iceland, Dept Elect & Comp Engn, Reykjavik, Iceland. EM benedikt@hi.is; sebastiano.serpico@unige.it; Jacqueline.LeMoigne@nasa.gov RI Benediktsson, Jon/F-2861-2010 OI Benediktsson, Jon/0000-0003-0621-9647 FU University of Iceland; NASA Goddard Space Flight Center FX This work was supported by the Research of Fund of the University of Iceland and was performed at NASA Goddard Space Flight Center. NR 13 TC 1 Z9 1 U1 0 U2 2 PU IEEE COMPUTER SOC PI LOS ALAMITOS PA 10662 LOS VAQUEROS CIRCLE, PO BOX 3014, LOS ALAMITOS, CA 90720-1264 USA BN 978-0-7695-3637-8 PY 2009 BP 211 EP + DI 10.1109/SMC-IT.2009.32 PG 3 WC Engineering, Aerospace SC Engineering GA BMO51 UT WOS:000273122700027 ER PT B AU Lim, CS Jain, A AF Lim, Christopher S. Jain, Abhinandan GP IEEE COMPUTER SOC TI Dshell plus plus : A Component Based, Reusable Space System Simulation Framework SO SMC-IT 2009: THIRD IEEE INTERNATIONAL CONFERENCE ON SPACE MISSION CHALLENGES FOR INFORMATION TECHNOLOGY, PROCEEDINGS LA English DT Proceedings Paper CT 3rd IEEE International Conference on Space Mission Challenges for Information Technology CY JUL 19-23, 2009 CL Pasadena, CA SP IEEE DE Aerospace simulation software AB This paper describes the multi-mission Dshell++ simulation framework for high fidelity, physics-based simulation of spacecraft, robotic manipulation and mobility systems. Dshell++ is a C++/Python library which uses modern script-driven object-oriented techniques to allow component reuse and a dynamic run-time interface for complex, high-fidelity simulation of spacecraft and robotic systems. The goal of the Dshell++ architecture is to manage the inherent complexity of physics-based simulations while supporting component model reuse across missions. The framework provides several features that support a large degree of simulation configurability and usability. C1 [Lim, Christopher S.; Jain, Abhinandan] CALTECH, Jet Prop Lab, Pasadena, CA 91009 USA. RP Lim, CS (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91009 USA. EM Christopher.S.Lim@jpl.nasa.gov NR 19 TC 0 Z9 0 U1 0 U2 0 PU IEEE COMPUTER SOC PI LOS ALAMITOS PA 10662 LOS VAQUEROS CIRCLE, PO BOX 3014, LOS ALAMITOS, CA 90720-1264 USA BN 978-0-7695-3637-8 PY 2009 BP 229 EP 236 DI 10.1109/SMC-IT.2009.35 PG 8 WC Engineering, Aerospace SC Engineering GA BMO51 UT WOS:000273122700030 ER PT B AU Pomerantz, MI Jain, A Myint, S AF Pomerantz, Marc I. Jain, Abhinandan Myint, Steven GP IEEE COMPUTER SOC TI Dspace: Real-time 3D Visualization System for Spacecraft Dynamics Simulation SO SMC-IT 2009: THIRD IEEE INTERNATIONAL CONFERENCE ON SPACE MISSION CHALLENGES FOR INFORMATION TECHNOLOGY, PROCEEDINGS LA English DT Proceedings Paper CT 3rd IEEE International Conference on Space Mission Challenges for Information Technology CY JUL 19-23, 2009 CL Pasadena, CA SP IEEE AB The multi-mission Dshell++ simulation framework has formed the basis for high-performance, physics-based simulations for a large variety of space mission simulations including cruise and orbiter spacecraft, Entry, Descent, Landing (EDL) missions as well as for planetary surface rovers. The Dspace interactive, reusable 3D visualization system has been developed to support the diverse visualization needs of such complex real-time simulations C1 [Pomerantz, Marc I.; Jain, Abhinandan; Myint, Steven] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Pomerantz, MI (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM Marc.I.Pomerantz@jpl.nasa.gov NR 16 TC 1 Z9 1 U1 0 U2 0 PU IEEE COMPUTER SOC PI LOS ALAMITOS PA 10662 LOS VAQUEROS CIRCLE, PO BOX 3014, LOS ALAMITOS, CA 90720-1264 USA BN 978-0-7695-3637-8 PY 2009 BP 237 EP 245 DI 10.1109/SMC-IT.2009.36 PG 9 WC Engineering, Aerospace SC Engineering GA BMO51 UT WOS:000273122700031 ER PT B AU Estlin, T Castano, R Bornstein, B Gaines, D Anderson, RC de Granville, C Thompson, D Burl, M Judd, M Chien, S AF Estlin, Tara Castano, Rebecca Bornstein, Benjamin Gaines, Daniel Anderson, Robert C. de Granville, Charles Thompson, David Burl, Michael Judd, Michele Chien, Steve GP IEEE COMPUTER SOC TI Automated Targeting for the MER Rovers SO SMC-IT 2009: THIRD IEEE INTERNATIONAL CONFERENCE ON SPACE MISSION CHALLENGES FOR INFORMATION TECHNOLOGY, PROCEEDINGS LA English DT Proceedings Paper CT 3rd IEEE International Conference on Space Mission Challenges for Information Technology CY JUL 19-23, 2009 CL Pasadena, CA SP IEEE AB The Autonomous Exploration for Gathering Increased Science System (AEGIS) will soon provide automated targeting for remote sensing instruments on the Mars Exploration Rover (MER) mission, which currently has two rovers exploring the surface of Mars. Targets for rover remote-sensing instruments, especially narrow field-of-view instruments (such as the MER Mini-TES spectrometer or the 2011 Mars Science Laboratory (MSL) Mission ChemCam Spectrometer), are typically selected manually based on imagery already on the ground with the operations team. AEGIS enables the rover flight software to analyze imagery onboard in order to autonomously select and sequence targeted remote-sensing observations in an opportunistic fashion In this paper, we first provide background information on the larger autonomous science framework in which AEGIS was developed. We then describe how AEGIS was specifically developed and tested on the JPL FIDO rover. Finally we discuss how AEGIS will be uploaded and used on the Mars Exploration Rover (MER) mission in mid 2009. C1 [Estlin, Tara; Castano, Rebecca; Bornstein, Benjamin; Gaines, Daniel; Anderson, Robert C.; de Granville, Charles; Thompson, David; Burl, Michael; Judd, Michele; Chien, Steve] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Estlin, T (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM tara.estlin@jpl.nasa.gov; rebecca.castano@jpl.nasa.gov; benjamin.bornstein@jpl.nasa.gov; daniel.gaines@jpl.nasa.gov; robert.anderson@jpl.nasa.gov; charles.degranville@jpl.nasa.gov; david.thompson@jpl.nasa.gov; michael.burl@jpl.nasa.gov; michele.judd@jpl.nasa.gov; steve.chien@jpl.nasa.gov NR 9 TC 0 Z9 0 U1 0 U2 2 PU IEEE COMPUTER SOC PI LOS ALAMITOS PA 10662 LOS VAQUEROS CIRCLE, PO BOX 3014, LOS ALAMITOS, CA 90720-1264 USA BN 978-0-7695-3637-8 PY 2009 BP 257 EP 263 DI 10.1109/SMC-IT.2009.38 PG 7 WC Engineering, Aerospace SC Engineering GA BMO51 UT WOS:000273122700033 ER PT B AU Gaines, D Estlin, T Schaffer, S Chouinard, C Elfes, A AF Gaines, Daniel Estlin, Tara Schaffer, Steve Chouinard, Caroline Elfes, Alberto GP IEEE COMPUTER SOC TI Autonomous Planning and Execution for a Future Titan Aerobot SO SMC-IT 2009: THIRD IEEE INTERNATIONAL CONFERENCE ON SPACE MISSION CHALLENGES FOR INFORMATION TECHNOLOGY, PROCEEDINGS LA English DT Proceedings Paper CT 3rd IEEE International Conference on Space Mission Challenges for Information Technology CY JUL 19-23, 2009 CL Pasadena, CA SP IEEE AB We are developing onboard planning and execution technologies to provide robust and opportunistic mission operations for a future Titan aerobot. Aerobot have the potential for collecting a vast amount of high priority science data. However, to be effective, an aerobot must address several challenges including communication constraints, extended periods without contact with Earth, uncertain and changing environmental conditions, maneuvarability constraints and potentially short-lived science opportunities. We are developing the AerOASIS system to develop and test technology to support autonomous science operations for a future Titan Aerobot. The planning and execution component of AerOASIS is able to generate mission operations plans that achieve science and engineering objectives while respecting mission and resource constraints as well as adapt the plan to respond to new science opportunities. Our technology leverages prior work on the OASIS system for autonomous rover exploration. In this paper we describe how the OASIS planning component was adapted to address the unique challenges of a Titan Aerobot and we describe a field demonstration of the system with the JPL prototype aerobot. C1 [Gaines, Daniel; Estlin, Tara; Schaffer, Steve; Chouinard, Caroline; Elfes, Alberto] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Gaines, D (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM daniel.gaines@jpl.nasa.gov; tara.estlin@jpl.nasa.gov; steve.schaffer@jpl.nasa.gov; caroline.chouinard@jpl.nasa.gov; alberto.elfes@jpl.nasa.gov RI Elfes, Alberto/E-2463-2011 OI Elfes, Alberto/0000-0003-2433-995X NR 8 TC 0 Z9 0 U1 0 U2 1 PU IEEE COMPUTER SOC PI LOS ALAMITOS PA 10662 LOS VAQUEROS CIRCLE, PO BOX 3014, LOS ALAMITOS, CA 90720-1264 USA BN 978-0-7695-3637-8 PY 2009 BP 264 EP 269 DI 10.1109/SMC-IT.2009.39 PG 6 WC Engineering, Aerospace SC Engineering GA BMO51 UT WOS:000273122700034 ER PT B AU Hanna, RA AF Hanna, Robert A. GP IEEE COMPUTER SOC TI Earned Value Management Software Projects SO SMC-IT 2009: THIRD IEEE INTERNATIONAL CONFERENCE ON SPACE MISSION CHALLENGES FOR INFORMATION TECHNOLOGY, PROCEEDINGS LA English DT Proceedings Paper CT 3rd IEEE International Conference on Space Mission Challenges for Information Technology CY JUL 19-23, 2009 CL Pasadena, CA SP IEEE DE Cost; Schedule; Software; Management AB JPL has been attempting to apply EVM techniques for the last 15 years with mixed success, especially when applied to software tasks. One of the main causes is that software presents particular challenges that were not considered during the genesis of EVM. A small number of tasks have been able to use EVM effectively and derive great benefits. This paper discusses challenges specific to software management and how they can be successfully addressed. Specifically, it details lessons learned from the $28 million dollar Next Generation Navigation Software Project that replaced NASA's deep space navigation software for operations. The project was able to successfully use EVM techniques during a four year period, producing 12 releases on their promised delivery dates and projects actual costs that were within 0.3% of the planned budget (under), in contrast to performance before the techniques were put into practice. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. RP Hanna, RA (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91125 USA. EM Robert.A.Hanna@jpl.nasa.gov NR 6 TC 2 Z9 2 U1 2 U2 3 PU IEEE COMPUTER SOC PI LOS ALAMITOS PA 10662 LOS VAQUEROS CIRCLE, PO BOX 3014, LOS ALAMITOS, CA 90720-1264 USA BN 978-0-7695-3637-8 PY 2009 BP 297 EP 304 DI 10.1109/SMC-IT.2009.42 PG 8 WC Engineering, Aerospace SC Engineering GA BMO51 UT WOS:000273122700038 ER PT B AU Fijany, A Barrett, A Vatan, F AF Fijany, Amir Barrett, Anthony Vatan, Farrokh GP IEEE COMPUTER SOC TI A Novel Efficient Method for Conflicts Set Generation for Model-Based Diagnosis SO SMC-IT 2009: THIRD IEEE INTERNATIONAL CONFERENCE ON SPACE MISSION CHALLENGES FOR INFORMATION TECHNOLOGY, PROCEEDINGS LA English DT Proceedings Paper CT 3rd IEEE International Conference on Space Mission Challenges for Information Technology CY JUL 19-23, 2009 CL Pasadena, CA SP IEEE DE model-based diagnosis; fault detection; conflict; analytical redundancy relation; hitting set problem ID ANALYTICAL REDUNDANCY RELATIONS AB In this paper we present a new efficient algorithmic method for generating the conflicts set for model-based diagnosis. Our new method combines the strength of the two different approaches proposed in the literature, that is, the Fault Detection and Isolation (FDI), which is based on automatic control theory and statistical decision theory, and the other one, known as DX, which is based on artificial intelligence techniques. The first building block in our method is a new efficient algorithm for generation of the complete set of Analytical redundancy Relations (ARRs) for the system in an implicit form. For the diagnosis, our method first performs (similar to DX approaches) a system simulation to calculate the expected values of the measurements. Any discrepancy, i.e., the difference between expected and actual value of measurement, would trigger our diagnosis process. To this end, only those ARRs which involve the measurement with discrepancy are checked for consistency which lead a to a significant reduction in the number of consistency checks usually performed by DX approaches. We demonstrate the efficiency of our new method by its application to several synthetic systems and compare it with that of GDE. C1 [Fijany, Amir] Italian Inst Technol, Genoa, Italy. [Barrett, Anthony; Vatan, Farrokh] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. RP Fijany, A (reprint author), Italian Inst Technol, Genoa, Italy. EM Amir.Fijany@iit.it; Anthony.C.Barrett@jpl.nasa.gov; Farrokh.Vatan@jpl.nasa.gov NR 9 TC 1 Z9 2 U1 0 U2 4 PU IEEE COMPUTER SOC PI LOS ALAMITOS PA 10662 LOS VAQUEROS CIRCLE, PO BOX 3014, LOS ALAMITOS, CA 90720-1264 USA BN 978-0-7695-3637-8 PY 2009 BP 346 EP + DI 10.1109/SMC-IT.2009.58 PG 2 WC Engineering, Aerospace SC Engineering GA BMO51 UT WOS:000273122700044 ER PT B AU Duong, TA Duong, VA AF Duong, Tuan A. Duong, Vu A. GP IEEE COMPUTER SOC TI Sequential Principal Component Analysis-A Hardware-Implementable Transform for Image Compression SO SMC-IT 2009: THIRD IEEE INTERNATIONAL CONFERENCE ON SPACE MISSION CHALLENGES FOR INFORMATION TECHNOLOGY, PROCEEDINGS LA English DT Proceedings Paper CT 3rd IEEE International Conference on Space Mission Challenges for Information Technology CY JUL 19-23, 2009 CL Pasadena, CA SP IEEE DE Sequential Principal Component Analysis; Image compression; JPEG2000; hardware implementation AB This paper presents the JPL-developed Sequential Principal Component Analysis (SPCA) algorithm for feature extraction / image compression, based on "dominant-term selection" unsupervised learning technique that requires an order-of-magnitude lesser computation and has simpler architecture compared to the state of the art gradient-descent techniques. This algorithm is inherently amenable to a compact, low power and high speed VLSI hardware embodiment. The paper compares the lossless image compression performance of the JPL's SPCA algorithm with the state of the art JPEG2000, widely used due to its simplified hardware implementability. JPEG2000 is not an optimal data compression technique because of its fixed transform characteristics, regardless of its data structure. On the other hand, conventional Principal Component Analysis based transform (PCA-transform) is a data-dependent-structure transform. However, it is not easy to implement the PCA in compact VLSI hardware, due to its highly computational and architectural complexity. In contrast, the JPL's "dominant-term selection" SPCA algorithm allows, for the first time, a compact, low-power hardware implementation of the powerful PCA algorithm. This paper presents a direct comparison of the JPL's SPCA versus JPEG2000, incorporating the Huffman and arithmetic coding for completeness of the data compression operation. The simulation results show that JPL's SPCA algorithm is superior as an optimal data-dependent-transform over the state of tire art JPEG2000. When implemented in hardware, this technique is projected to be ideally suited to future NASA missions for autonomous on-board image data processing to improve the bandwidth of communication. C1 [Duong, Tuan A.; Duong, Vu A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Duong, TA (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM taduong@jpl.nasa.gov; vaduong@jpl.nasa.gov NR 17 TC 0 Z9 0 U1 0 U2 0 PU IEEE COMPUTER SOC PI LOS ALAMITOS PA 10662 LOS VAQUEROS CIRCLE, PO BOX 3014, LOS ALAMITOS, CA 90720-1264 USA BN 978-0-7695-3637-8 PY 2009 BP 362 EP 366 DI 10.1109/SMC-IT.2009.49 PG 5 WC Engineering, Aerospace SC Engineering GA BMO51 UT WOS:000273122700046 ER PT B AU Daugherty, SC Cervantes, BW AF Daugherty, Sarah C. Cervantes, Benjamin W. GP IEEE COMPUTER SOC TI The Mission Planning Lab: A Visualization and Analysis Tool SO SMC-IT 2009: THIRD IEEE INTERNATIONAL CONFERENCE ON SPACE MISSION CHALLENGES FOR INFORMATION TECHNOLOGY, PROCEEDINGS LA English DT Proceedings Paper CT 3rd IEEE International Conference on Space Mission Challenges for Information Technology CY JUL 19-23, 2009 CL Pasadena, CA SP IEEE DE modeling; simulation; software integration; visualization AB Simulation and visualization are powerful decision making tools that are time-saving and cost-effiective. Space missions pose testing and evaluation challenges that can be overcome through modeling, simulation, and visualization Of mission parameters. The National Aeronautics and Space Administration's (NASA) Wallops Flight Facility (WFF) capitalizes on the benefits of modeling, simulation, and visualization tools through a project initiative called The Mission Planning Lab (MPL). C1 [Daugherty, Sarah C.; Cervantes, Benjamin W.] NASA, Wallops Flight Facil, Wallops Syst Software Engn Branch, Wallops Isl, VA USA. RP Daugherty, SC (reprint author), NASA, Wallops Flight Facil, Wallops Syst Software Engn Branch, Wallops Isl, VA USA. EM Sarah.C.Daugherty@nasa.gov; Benjamin.W.Cervantes@nasa.gov NR 0 TC 0 Z9 0 U1 0 U2 0 PU IEEE COMPUTER SOC PI LOS ALAMITOS PA 10662 LOS VAQUEROS CIRCLE, PO BOX 3014, LOS ALAMITOS, CA 90720-1264 USA BN 978-0-7695-3637-8 PY 2009 BP 369 EP 375 DI 10.1109/SMC-IT.2009.51 PG 7 WC Engineering, Aerospace SC Engineering GA BMO51 UT WOS:000273122700047 ER PT B AU Barrett, A Dvorak, D AF Barrett, Anthony Dvorak, Daniel GP IEEE COMPUTER SOC TI A Combinatorial Test Suite Generator for Gray-Box Testing SO SMC-IT 2009: THIRD IEEE INTERNATIONAL CONFERENCE ON SPACE MISSION CHALLENGES FOR INFORMATION TECHNOLOGY, PROCEEDINGS LA English DT Proceedings Paper CT 3rd IEEE International Conference on Space Mission Challenges for Information Technology CY JUL 19-23, 2009 CL Pasadena, CA SP IEEE DE software testing; combinatorial testing; gray-box testing ID DESIGN AB In black-box testing, the system being tested is typically characterized as a number of inputs, where each input can take one of a number of values. Thus each test is a vector of input settings, and the set of possible tests is an N dimensional space, where N is the number of inputs. For example, an instance of a simulation of a Crew Exploration Vehicle's (CEV) launch pad abort scenario can have 76 floating-point inputs. Unfortunately, for such a large number of inputs only a small percentage of the test space can be actually tested. This paper characterizes levels of partial test space coverage and presents Testgen, a tool for generating a suite of tests that guarantees a level of test space coverage, which a user can adapt to take advantage of knowledge of system internals. This ability to adapt coverage makes Testgen a gray-box testing tool. C1 [Barrett, Anthony; Dvorak, Daniel] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. RP Barrett, A (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. EM anthony.barrett@jpl.nasa.gov; daniel.dvorak@jpl.nasa.gov NR 16 TC 3 Z9 3 U1 0 U2 1 PU IEEE COMPUTER SOC PI LOS ALAMITOS PA 10662 LOS VAQUEROS CIRCLE, PO BOX 3014, LOS ALAMITOS, CA 90720-1264 USA BN 978-0-7695-3637-8 PY 2009 BP 387 EP 393 DI 10.1109/SMC-IT.2009.53 PG 7 WC Engineering, Aerospace SC Engineering GA BMO51 UT WOS:000273122700049 ER PT B AU Nikora, AP Balcom, G AF Nikora, Allen P. Balcom, Galen GP IEEE COMPUTER SOC TI Improving the Accuracy of Space Mission Software Anomaly Frequency Estimates SO SMC-IT 2009: THIRD IEEE INTERNATIONAL CONFERENCE ON SPACE MISSION CHALLENGES FOR INFORMATION TECHNOLOGY, PROCEEDINGS LA English DT Proceedings Paper CT 3rd IEEE International Conference on Space Mission Challenges for Information Technology CY JUL 19-23, 2009 CL Pasadena, CA SP IEEE DE error estimation; failure analysis; software reliability; text processing AB Anomaly data can be used to estimate baseline values for operational mission software anomaly frequencies; these estimates can be used for future missions to determine whether software reliability is improving. The accuracy of anomaly frequency estimates can be affected by characteristics of the anomaly data and the problem reporting system maintaining that data. We have been using text mining and machine learning techniques to address one of these issues, in which the number of software-related anomalies is incorrectly reported because the problem reporting system does not tag them correctly. Results to date indicate that these techniques may substantially increase the accuracy of anomaly frequency estimates. C1 [Nikora, Allen P.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. [Balcom, Galen] Calif State Univ Fresno, Dept Comp Sci, Fresno, CA 93740 USA. RP Nikora, AP (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM Allen.P.Nikora@jpl.nasa.gov; gbalcom@csufresno.edu NR 17 TC 0 Z9 0 U1 0 U2 0 PU IEEE COMPUTER SOC PI LOS ALAMITOS PA 10662 LOS VAQUEROS CIRCLE, PO BOX 3014, LOS ALAMITOS, CA 90720-1264 USA BN 978-0-7695-3637-8 PY 2009 BP 402 EP + DI 10.1109/SMC-IT.2009.55 PG 3 WC Engineering, Aerospace SC Engineering GA BMO51 UT WOS:000273122700051 ER PT J AU Yasunari, TJ Yamazaki, K AF Yasunari, Teppei J. Yamazaki, Koji TI Origins of Air Masses over an Alaskan Glacier and Implications for Ice Core Studies in the North Pacific Region SO SOLA LA English DT Article ID STRATOSPHERE; CLIMATE; AEROSOLS; CANADA; YUKON; DUST AB Simulations of 10-day backward trajectories of air masses from Mount Wrangell, an Alaskan ice core site, were calculated for 11 years on a daily basis. Results were analyzed statistically in order to interpret monthly air mass contributions over the ice core site and to discuss implications for ice core studies in the North Pacific Region (NPR). Increases in tropospheric air mass transport from EA in spring suggest favorable transport conditions for Asian dust during this season. The stratospheric air mass (< 300 hPa) over the ice core site increases in winter and that from East Asia (EA) to the North Pacific Ocean in late spring. The tritium peaks observed in the ice core in late spring were discussed in the context of the present results with two possibilities on the time lag of tritium transportation in the stratosphere and the seasonal variations of water vapor amount in the troposphere. Increases in air masses originating from Siberia, Alaska and Canada in summer-fall favor the transport of black carbon due to forest fires over the ice core site. These results allow advanced interpretation of the origin and transport processes of materials in the ice core proxies in the NPR. C1 [Yasunari, Teppei J.] NASA, Goddard Space Flight Ctr, GEST, UMBC, Greenbelt, MD 20771 USA. [Yamazaki, Koji] Hokkaido Univ, Grad Sch Environm Sci, Sapporo, Hokkaido, Japan. RP Yasunari, TJ (reprint author), NASA, Goddard Space Flight Ctr, Climate & Radiat Branch, UMBC,GEST Ctr, Code 613-2, Greenbelt, MD 20771 USA. EM tj.yasunari@gmail.com RI Yasunari, Teppei/E-5374-2010 OI Yasunari, Teppei/0000-0002-9896-9404 NR 26 TC 5 Z9 5 U1 0 U2 5 PU METEOROLOGICAL SOC JPN PI TOKYO PA C/O JPN METEOROL AGENCY 1-3-4 OTE-MACHI, CHIYODA-KU, TOKYO, 100-0004, JAPAN SN 1349-6476 J9 SOLA JI SOLA PY 2009 VL 5 BP 77 EP 80 DI 10.2151/sola.2009-020 PG 4 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 545PG UT WOS:000273746300020 ER PT J AU Irie, H Kanaya, Y Takashima, H Gleason, JF Wang, ZF AF Irie, Hitoshi Kanaya, Yugo Takashima, Hisahiro Gleason, James F. Wang, Zifa TI Characterization of OMI Tropospheric NO2 Measurements in East Asia Based on a Robust Validation Comparison SO SOLA LA English DT Article ID MAX-DOAS AB In the period from June 2006 to December 2008, we measured the tropospheric nitrogen dioxide (NO2) column by ground-based Multi-Axis Differential Optical Absorption Spectroscopy (MAX-DOAS) at an urban site in China (Tai'an) and three sites in Japan, covering urban (Yokosuka), suburban (Tsukuba), and remote areas (Hedo). This robust dataset is used to characterize Ozone Monitoring Instrument (OMI) tropospheric NO2 column data (the standard product, version 3). Correlations between MAX-DOAS and OMI data, both of which show very low NO2 at Hedo and moderate/high levels at the other sites, have correlation coefficients (R-2) as high as 0.64, indicating that relative changes in OMI NO2 data are reliable. However, OMI data have a negative bias of 31% on average. Assuming that these results are valid for OMI data taken over China, we find an increasing trend in tropospheric column NO2 at about 5% per year on average in the industrial areas of China (30 degrees-40 degrees N and 110 degrees-123 degrees E) over 2005. 2008, but its spatial distribution is highly inhomogeneous. C1 [Irie, Hitoshi; Kanaya, Yugo; Takashima, Hisahiro] JAMSTEC, Res Inst Global Change, Yokohama, Kanagawa, Japan. [Gleason, James F.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Wang, Zifa] Chinese Acad Sci, Inst Atmospher Phys, Beijing, Peoples R China. RP Irie, H (reprint author), Japan Agcy Marine Earth Sci & Technol, Res Inst Global Change, Kanazawa Ku, 3173-25 Showa Machi, Kanagawa 2360001, Japan. EM irie@jamstec.go.jp RI Kanaya, Yugo/C-7446-2012; Wang, ZF/D-7202-2012; Gleason, James/E-1421-2012; Wang, Zifa/B-5799-2011 OI Wang, ZF/0000-0002-7062-6012; FU Ministry of Education, Culture, Sports, Science and Technology (MEXT); Ministry of the Environment, Japan [S-7] FX We thank PREDE, Co., Ltd for their technical assistance in developing the MAX-DOAS instruments. We are grateful to NIES for supporting measurements at Tsukuba and Hedo. This work was supported by the Japan EOS (Earth Observation System) Promotion Program of the Ministry of Education, Culture, Sports, Science and Technology (MEXT). This work was supported by the Global Environment Research Fund (S-7) of the Ministry of the Environment, Japan. NR 14 TC 11 Z9 13 U1 1 U2 8 PU METEOROLOGICAL SOC JPN PI TOKYO PA C/O JPN METEOROL AGENCY 1-3-4 OTE-MACHI, CHIYODA-KU, TOKYO, 100-0004, JAPAN SN 1349-6476 J9 SOLA JI SOLA PY 2009 VL 5 BP 117 EP 120 DI 10.2151/sola.2009-030 PG 4 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 545PG UT WOS:000273746300030 ER PT B AU Zhao, J Hartlep, T Kosovichev, AG Mansour, NN AF Zhao, J. Hartlep, T. Kosovichev, A. G. Mansour, N. N. BE Dikpati, M Arentoft, T Hernandez, IG Lindsey, C Hill, F TI Time-Distance Helioseismic Imaging of a Numerically Simulated Solar Tachocline SO SOLAR-STELLAR DYNAMOS AS REVEALED BY HELIO AND ASTEROSEISMOLOGY: GONG 2008/SOHO 21 SE Astronomical Society of the Pacific Conference Series LA English DT Proceedings Paper CT Workshop on Solar-Stellar Dynamos as Revealed by Helio and Asteroseismology (GONG 2008/SOHO 21) CY AUG 11-15, 2008 CL High Altitude Observ, Boulder, CO HO High Altitude Observ ID ROTATION; INTERIOR AB The solar tachocline, located near the bottom of the convection zone, is a very important region for solar dynamics and the solar dynamo. We develop a time-distance helioseismology technique, including both surface- and deep-focusing measurements, together with inversions, to derive the interior image of the sound speed perturbation at the tachocline with a latitudinal dependence. We test the technique on numerically simulated global wavefields and find that the technique is able to recover the major features that are preset in the numerical model, though a bit more widespread into the deeper interior. This measurement and inversion technique will be applied to MDI observations to derive the structures of solar tachocline. C1 [Zhao, J.; Kosovichev, A. G.] Stanford Univ, WW Hansen Expt Phys Lab, Room 130-452 Lomita Mall, Stanford, CA 94305 USA. [Hartlep, T.; Mansour, N. N.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Zhao, J (reprint author), Stanford Univ, WW Hansen Expt Phys Lab, Room 130-452 Lomita Mall, Stanford, CA 94305 USA. EM junwei@solar.stanford.edu; thartlep@solar.stanford.edu; akosovichev@solar.stanford.edu NR 10 TC 0 Z9 0 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 978-1-58381-712-4 J9 ASTR SOC P PY 2009 VL 416 BP 25 EP + PG 2 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BQL27 UT WOS:000281240900003 ER PT B AU Jacoutot, L Kosovichev, A Wray, A Mansour, N AF Jacoutot, L. Kosovichev, A. Wray, A. Mansour, N. BE Dikpati, M Arentoft, T Hernandez, IG Lindsey, C Hill, F TI Realistic MHD Simulations of Solar Convection and Oscillations in Magnetic Regions: Mode Excitation and Effects of Acoustic Halos SO SOLAR-STELLAR DYNAMOS AS REVEALED BY HELIO AND ASTEROSEISMOLOGY: GONG 2008/SOHO 21 SE Astronomical Society of the Pacific Conference Series LA English DT Proceedings Paper CT Workshop on Solar-Stellar Dynamos as Revealed by Helio and Asteroseismology (GONG 2008/SOHO 21) CY AUG 11-15, 2008 CL High Altitude Observ, Boulder, CO HO High Altitude Observ ID P-MODES; TURBULENT CONVECTION; RADIAL OSCILLATIONS; SUN AB We have used a 3D, compressible, non-linear radiative magnetohydrodynamics code developed at the NASA Ames Research Center to model solar convection and oscillations in magnetic regions. This code takes into account several physical phenomena: compressible fluid flow in a highly stratified medium, sub-grid scale turbulence models, radiative energy transfer, and a real-gas equation of state. We have studied the influence of the magnetic field of various strength on the convective cells and on the excitation mechanisms of the acoustic oscillations by calculating spectral properties of the convective motions and oscillations. The results reveal substantial changes of the granulation structure with increased magnetic field, and a frequency-dependent reduction in the oscillation power in a good agreement with solar observations. The simulations provide a solution to the long-standing problem of enhanced high-frequency acoustic emission at the boundaries of active region ("acoustic halos"), suggesting that this phenomenon is caused by the changes of the spatial-temporal spectrum of the turbulent convection in magnetic field, resulting in turbulent motions of smaller scales and higher frequencies than in quiet Sun regions. These simulation results may have also important implications for understanding high-frequency oscillations of magnetic stars. C1 [Jacoutot, L.] Stanford Univ, Ctr Turbulence Res, Stanford, CA 94305 USA. [Kosovichev, A.] Stanford Univ, HEPL, Stanford, CA 94305 USA. [Wray, A.; Mansour, N.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Jacoutot, L (reprint author), Stanford Univ, Ctr Turbulence Res, Stanford, CA 94305 USA. EM akosovichev@solar.stanford.edu NR 17 TC 1 Z9 1 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 978-1-58381-712-4 J9 ASTR SOC P PY 2009 VL 416 BP 67 EP + PG 3 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BQL27 UT WOS:000281240900009 ER PT B AU Duvall, TL Hanasoge, SM AF Duvall, T. L., Jr. Hanasoge, S. M. BE Dikpati, M Arentoft, T Hernandez, IG Lindsey, C Hill, F TI Measuring Meridional Circulation in the Sun SO SOLAR-STELLAR DYNAMOS AS REVEALED BY HELIO AND ASTEROSEISMOLOGY: GONG 2008/SOHO 21 SE Astronomical Society of the Pacific Conference Series LA English DT Proceedings Paper CT Workshop on Solar-Stellar Dynamos as Revealed by Helio and Asteroseismology (GONG 2008/SOHO 21) CY AUG 11-15, 2008 CL High Altitude Observ, Boulder, CO HO High Altitude Observ ID TIME-DISTANCE HELIOSEISMOLOGY AB Measuring the depth variation of the meridional flows is important for understanding the solar cycle, at least according to a number of dynamo models. While attempting to extend the early observations of Giles (2000) of time-distance measurements of flow, we have stumbled upon some systematic errors that can affect these measurements: 1) the additional distance traveled by radiation coming from points away from disk center causes an apparent 'shrinking' Sun, that is an apparent flow towards the disk center and 2) in measurements away from the central longitude, the rotation signal can leak into meridional flow signals. Attempts to understand and overcome these systematic problems will be presented. Forward models based on ray theory have been applied in order to test the sensitivity of travel times to various models. C1 [Duvall, T. L., Jr.] NASA, Goddard Space Flight Ctr, Solar Phys Lab, Greenbelt, MD 20771 USA. [Hanasoge, S. M.] Stanford Univ, W W 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 tduvall@solar.stanford.edu; hanasoge@gmail.com RI Duvall, Thomas/C-9998-2012 NR 11 TC 11 Z9 11 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 978-1-58381-712-4 J9 ASTR SOC P PY 2009 VL 416 BP 103 EP + PG 3 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BQL27 UT WOS:000281240900015 ER PT B AU Beck, JG Duvall, TL Zhao, J AF Beck, J. G. Duvall, T. L., Jr. Zhao, J. BE Dikpati, M Arentoft, T Hernandez, IG Lindsey, C Hill, F TI Travel-Time Errors Due To Data Gaps SO SOLAR-STELLAR DYNAMOS AS REVEALED BY HELIO AND ASTEROSEISMOLOGY: GONG 2008/SOHO 21 SE Astronomical Society of the Pacific Conference Series LA English DT Proceedings Paper CT Workshop on Solar-Stellar Dynamos as Revealed by Helio and Asteroseismology (GONG 2008/SOHO 21) CY AUG 11-15, 2008 CL High Altitude Observ, Boulder, CO HO High Altitude Observ AB Time-distance measurements of wave packet travel times can be used to determine various properties of the plasma through which the p modes propagate, however, missing data can introduce significant errors in the travel time measurements. We find that the magnitude of the error depends on the amount of missing data, the temporal position of the data gaps, and the travel distance, but not on the continuity of data gaps. Further, apodizing the data gaps or linearly filling the gaps fails to reduce the errors. C1 [Beck, J. G.] Stanford Univ, WW Hansen Expt Phys Lab, Stanford Solar Observ, Room 130-452 Lomita Mall, Stanford, CA 94305 USA. [Duvall, T. L., Jr.] NASA, Goddard Space Flight Ctr, Astron & Solar Phys Lab, Greenbelt, MD 20771 USA. RP Beck, JG (reprint author), Stanford Univ, WW Hansen Expt Phys Lab, Stanford Solar Observ, Room 130-452 Lomita Mall, Stanford, CA 94305 USA. EM jbeck@solar.stanford.edu; tduvall@solar.stanford.edu; junwei@solar.stanford.edu RI Duvall, Thomas/C-9998-2012 FU NASA [NAG5-8878] FX This work was supported by NASA grant NAG5-8878. NR 3 TC 0 Z9 0 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 978-1-58381-712-4 J9 ASTR SOC P PY 2009 VL 416 BP 135 EP + PG 2 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BQL27 UT WOS:000281240900022 ER PT B AU Hartlep, T Kosovichev, AG Zhao, J Mansour, NN AF Hartlep, T. Kosovichev, A. G. Zhao, J. Mansour, N. N. BE Dikpati, M Arentoft, T Hernandez, IG Lindsey, C Hill, F TI Signatures of Emerging Subsurface Structures in Acoustic Power Maps SO SOLAR-STELLAR DYNAMOS AS REVEALED BY HELIO AND ASTEROSEISMOLOGY: GONG 2008/SOHO 21 SE Astronomical Society of the Pacific Conference Series LA English DT Proceedings Paper CT Workshop on Solar-Stellar Dynamos as Revealed by Helio and Asteroseismology (GONG 2008/SOHO 21) CY AUG 11-15, 2008 CL High Altitude Observ, Boulder, CO HO High Altitude Observ ID NUMERICAL SIMULATIONS; SOLAR; SUN AB We show that under suitable conditions subsurface structures can alter the average acoustic power observed at the photosphere. By using numerical simulations of wave propagation, we investigate whether this effect can be used to detect emerging active regions before they appear on the surface. In the simulations, subsurface structures are modeled as regions with enhanced or reduced acoustic wave speed. We show how the acoustic power above a subsurface region depends on the sign, depth and strength of the wave speed perturbation. For comparison, we analyze observations from SOHO/MDI of the emergence of active region NOAA 10488. C1 [Hartlep, T.] Stanford Univ, Ctr Turbulence Res, Stanford, CA 94305 USA. [Kosovichev, A. G.; Zhao, J.] Stanford Univ, W W Hansen Expt Phys, Stanford, CA 94305 USA. [Mansour, N. N.] NASA Ames Res Ctr, Moffett Field, CA USA. RP Hartlep, T (reprint author), Stanford Univ, Ctr Turbulence Res, Stanford, CA 94305 USA. EM thartlep@solar.stanford.edu; akosovichev@solar.stanford.edu; junwei@solar.stanford.edu NR 8 TC 0 Z9 0 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 978-1-58381-712-4 J9 ASTR SOC P PY 2009 VL 416 BP 147 EP + PG 2 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BQL27 UT WOS:000281240900025 ER PT B AU Ilonidis, S Zhao, J Hartlep, T AF Ilonidis, S. Zhao, J. Hartlep, T. BE Dikpati, M Arentoft, T Hernandez, IG Lindsey, C Hill, F TI Time-Distance Solar Far-Side Imaging Using Three-Skip Acoustic Signals SO SOLAR-STELLAR DYNAMOS AS REVEALED BY HELIO AND ASTEROSEISMOLOGY: GONG 2008/SOHO 21 SE Astronomical Society of the Pacific Conference Series LA English DT Proceedings Paper CT Workshop on Solar-Stellar Dynamos as Revealed by Helio and Asteroseismology (GONG 2008/SOHO 21) CY AUG 11-15, 2008 CL High Altitude Observ, Boulder, CO HO High Altitude Observ ID SUN AB The purpose of this work is to image the solar far-side active regions using acoustic signals with three skips. The mapping of the far-side active regions was first made possible (Lindsey & Braun 2000) using helioseismic holography technique by use of four-skip acoustic signals. The quality of far-side images was later improved with the combination of four- and five-skip signals using the time-distance technique (Zhao 2007). In this work, we further explore the possibility of making three-skip far-side images of active regions, and improving the image quality by combining the three-skip images with the images obtained from existing techniques. C1 [Ilonidis, S.; Zhao, J.] Stanford Univ, WW Hansen Expt Phys Lab, Stanford, CA 94305 USA. [Zhao, J.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Hartlep, T.] Stanford Univ, W W Hansen Expt Phys Lab, Stanford, CA 94305 USA. RP Ilonidis, S (reprint author), Stanford Univ, WW Hansen Expt Phys Lab, Stanford, CA 94305 USA. EM ilonidis@solar.stanford.edu; junwei@solar.stanford.edu; thartlep@solar.stanford.edu FU NASA Living With a Star program and the NASA Postdoctoral Program administered by Oak Ridge Associated Universities under contract with NASA FX The numerical simulations used in this paper were performed at NASA Ames Research Center. T.H. was supported by the NASA Living With a Star program and the NASA Postdoctoral Program administered by Oak Ridge Associated Universities under contract with NASA. NR 8 TC 0 Z9 0 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 978-1-58381-712-4 J9 ASTR SOC P PY 2009 VL 416 BP 163 EP + PG 2 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BQL27 UT WOS:000281240900029 ER PT B AU Hathaway, DH Williams, PE Cuntz, M AF Hathaway, D. H. Williams, P. E. Cuntz, M. BE Dikpati, M Arentoft, T Hernandez, IG Lindsey, C Hill, F TI The Advection of Supergranules by Large-Scale Flows SO SOLAR-STELLAR DYNAMOS AS REVEALED BY HELIO AND ASTEROSEISMOLOGY: GONG 2008/SOHO 21 SE Astronomical Society of the Pacific Conference Series LA English DT Proceedings Paper CT Workshop on Solar-Stellar Dynamos as Revealed by Helio and Asteroseismology (GONG 2008/SOHO 21) CY AUG 11-15, 2008 CL High Altitude Observ, Boulder, CO HO High Altitude Observ ID SPHERICAL HARMONIC-ANALYSIS; STEADY PHOTOSPHERIC FLOWS; MICHELSON DOPPLER IMAGER; SOLAR PHOTOSPHERE; VELOCITY-FIELDS; ROTATION AB We produce a 10-day series of simulated Doppler images at a 15-minute cadence that reproduces the spatial and temporal characteristics seen in the SOHO/MDI Doppler data. Our simulated data contains a spectrum of cellular flows with but two necessary components-a granule component that peaks at wavenumbers of about 4000 and a supergranule component that peaks at wavenumbers of about 110. We include the advection of these cellular components by a differential rotation profile that depends on latitude and wavenumber (depth). We further mimic the evolution of the cellular pattern by introducing random variations to the amplitudes and phases of the spectral components at rates that reproduce the level of cross-correlation as a function of time and latitude. Our simulated data do not include any wave-like characteristics for the supergranules yet can accurately reproduce the rotation characteristics previously attributed to wave-like characteristics. C1 [Hathaway, D. H.] NASA, George C Marshall Space Flight Ctr, Code ES-82, Huntsville, AL 35812 USA. [Williams, P. E.; Cuntz, M.] Univ Texas Arlington, Dept Phys, Arlington, TX 76019 USA. RP Hathaway, DH (reprint author), NASA, George C Marshall Space Flight Ctr, Code ES-82, Huntsville, AL 35812 USA. EM david.hathaway@msfc.nasa.gov FU NASA Marshall Space Flight Center; University of Texas Arlington FX We would like to thank NASA for its support of this research through a grant from the Heliophysics Guest Investigator Program to NASA Marshall Space Flight Center and The University of Texas Arlington. We would also like to thank the SOHO/MDI team for the critical role they played in producing the raw MDI data and John Beck in particular for implementing the temporal averaging of that data to remove the p-mode noise. NR 18 TC 0 Z9 0 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 978-1-58381-712-4 J9 ASTR SOC P PY 2009 VL 416 BP 495 EP + PG 2 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BQL27 UT WOS:000281240900086 ER PT B AU Svanda, M Kosovichev, AG Klvana, M Sobotka, M Duvall, TL AF Svanda, M. Kosovichev, A. G. Klvana, M. Sobotka, M. Duvall, T. L., Jr. BE Dikpati, M Arentoft, T Hernandez, IG Lindsey, C Hill, F TI Transport of Supergranules and their Vertical Coherence SO SOLAR-STELLAR DYNAMOS AS REVEALED BY HELIO AND ASTEROSEISMOLOGY: GONG 2008/SOHO 21 SE Astronomical Society of the Pacific Conference Series LA English DT Proceedings Paper CT Workshop on Solar-Stellar Dynamos as Revealed by Helio and Asteroseismology (GONG 2008/SOHO 21) CY AUG 11-15, 2008 CL High Altitude Observ, Boulder, CO HO High Altitude Observ ID TIME-DISTANCE HELIOSEISMOLOGY; SOLAR SUPERGRANULATION; FLOWS AB In recent papers, we have introduced a method for measuring the photospheric flow field that is based on the tracking of supergranular structures. Here, in combination with helioseismic data, we are able to estimate the depth in the solar convection envelope to which the detected large-scale flow field is coherent. We show that the upper 10 Mm in the convection zone depicts similar features in horizontal velocity. Our interpretation of this observation is that the supergranulation is a coherent structure 10 Mm deep and is subject to large-scale transport by the underlying velocity field. C1 [Svanda, M.] Charles Univ Prague, Astron Inst, V Holesovickach 2, Prague, Czech Republic. [Svanda, M.; Klvana, M.; Sobotka, M.] NASA, Goddard Space Flight Ctr, Solar Phys Lab, CZ-25165 Ondrejov, Czech Republic. [Kosovichev, A. G.] Stanford Univ, HEPL, Stanford, CA 94305 USA. [Duvall, T. L., Jr.] NASA, Goddard Space Flight Ctr, Astron & Solar Phys Lab, Greenbelt, MD 20771 USA. RP Svanda, M (reprint author), Charles Univ Prague, Astron Inst, V Holesovickach 2, Prague, Czech Republic. EM akosovichev@solar.stanford.edu; tduvall@solar.stanford.edu RI Svanda, Michal/A-6576-2008; Duvall, Thomas/C-9998-2012; Sobotka, Michal/G-9042-2014 OI Svanda, Michal/0000-0002-6345-1007; Sobotka, Michal/0000-0001-5439-7822 FU Agency of Academy of Science of the Czech Republic [IAA30030808]; Astronomical Institute of Charles University [MSM0021620860]; Ministry of Education of CR FX M.S, M. K.,and M. S. were supported by the Grant Agency of Academy of Science of the Czech Republic under grant IAA30030808. The Astronomical Institute of Charles University works on the Research program MSM0021620860 (Ministry of Education of CR). NR 7 TC 1 Z9 1 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 978-1-58381-712-4 J9 ASTR SOC P PY 2009 VL 416 BP 547 EP + PG 2 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BQL27 UT WOS:000281240900095 ER PT S AU Prasad, NS Trivedi, S Kutcher, S Wang, CC Kim, JS Hommerich, U Shukla, V Sadangi, R AF Prasad, Narasimha S. Trivedi, Sudhir Kutcher, Susan Wang, Chen-Chia Kim, Joo-Soo Hommerich, Uwe Shukla, Vijay Sadangi, Rajendra BE Clarkson, WA Hodgson, N Shori, RK TI Development of ceramic solid-state laser host materials SO SOLID STATE LASERS XVIII: TECHNOLOGY AND DEVICES SE Proceedings of SPIE-The International Society for Optical Engineering LA English DT Proceedings Paper CT Conference on Solid State Lasers XVIII - Technology and Devices CY JAN 25-29, 2009 CL San Jose, CA SP SPIE, Coherent, Inc DE Solid-state lasers; ceramic laser host materials; Neodymium doped Yttria; Ytterbium Yttria; Erbium Yttria; Scandium Oxide; Lutesium Oxide ID TRANSFORMATION-ASSISTED CONSOLIDATION AB Polycrystalline ceramic laser materials are gaining importance in the development of novel diode-pumped solid-state lasers. Compared to single-crystals, ceramic laser materials offer advantages in terms of ease of fabrication, shape, size, and control of dopant concentrations. Recently, we have developed Neodymium doped Yttria (Nd:Y(2)O(3)) as a solid-state ceramic laser material. A scalable production method was utilized to make spherical non agglomerated and monodisperse metastable ceramic powders of compositions that were used to fabricate polycrystalline ceramic material components. This processing technique allowed for higher doping concentrations without the segregation problems that are normally encountered in single crystalline growth. We have successfully fabricated undoped and Neodymium doped Yttria material up to 2 '' in diameter, Ytterbium doped Yttria, and erbium doped Yttria. We are also in the process of developing other sesquioxides such as scandium Oxide (Sc(2)O(3)) and Lutesium Oxide (Lu(2)O(3)) doped with Ytterbium, erbium and thulium dopants. In this paper, we present our initial results on the material, optical, and spectroscopic properties of the doped and undoped sesquioxide materials. Polycrystalline ceramic lasers have enormous potential applications including remote sensing, chem.-bio detection, and space exploration research. It is also potentially much less expensive to produce ceramic laser materials compared to their single crystalline counterparts because of the shorter fabrication time and the potential for mass production in large sizes. C1 [Prasad, Narasimha S.] NASA, Langley Res Ctr, Laser Remote Sensing Branch, Hampton, VA 23681 USA. RP Prasad, NS (reprint author), NASA, Langley Res Ctr, Laser Remote Sensing Branch, 5 N Dryden St,MS 468, Hampton, VA 23681 USA. EM Narasimha.s.prasad@nasa.gov NR 6 TC 0 Z9 0 U1 0 U2 6 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 978-0-8194-7439-1 J9 P SOC PHOTO-OPT INS PY 2009 VL 7193 AR 71931X DI 10.1117/12.813785 PG 11 WC Instruments & Instrumentation; Optics SC Instruments & Instrumentation; Optics GA BSL69 UT WOS:000284870500055 ER PT S AU Prasad, NS AF Prasad, Narasimha S. BE Clarkson, WA Hodgson, N Shori, RK TI Some Activities of MISSE 6 Mission SO SOLID STATE LASERS XVIII: TECHNOLOGY AND DEVICES SE Proceedings of SPIE LA English DT Proceedings Paper CT Conference on Solid State Lasers XVIII - Technology and Devices CY JAN 25-29, 2009 CL San Jose, CA SP SPIE, Coherent Inc DE MISSE 6; Space Qualification; Laser components; International Space Station; STS-123 AB The objective of the Materials International Space Station Experiment (MISSE) is to study the performance of novel materials when subjected to the synergistic effects of the harsh space environment for several months. In this paper, a few laser and optical elements from NASA Langley Research Center (LaRC) that have been flown on MISSE 6 mission will be discussed. These items were characterized and packed inside a ruggedized Passive Experiment Container (PEC) that resembles a suitcase. The PEC was tested for survivability due to launch conditions. Subsequently, the MISSE 6 PEC was transported by the STS-123 mission to International Space Station (ISS) on March 11, 2008. The astronauts successfully attached the PEC to external handrails and opened the PEC for long term exposure to the space environment. The plan is to retrieve the MISSE 6 PEC by STS-128 mission in August 2009. C1 NASA, Langley Res Ctr, Hampton, VA 23681 USA. RP Prasad, NS (reprint author), NASA, Langley Res Ctr, 5 N Dryden St,MS 468, Hampton, VA 23681 USA. EM narasimha.s.prasad@nasa.gov NR 7 TC 0 Z9 0 U1 0 U2 1 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 978-0-8194-7439-1 J9 PROC SPIE PY 2009 VL 7193 AR 719304 DI 10.1117/12.814870 PG 7 WC Instruments & Instrumentation; Optics SC Instruments & Instrumentation; Optics GA BSL69 UT WOS:000284870500001 ER PT S AU Shaw, GB Stephen, MA Troupaki, E Vasilyev, AA Yu, AW AF Shaw, George B. Stephen, Mark A. Troupaki, Elisavet Vasilyev, Aleksey A. Yu, Anthony W. BE Clarkson, WA Hodgson, N Shori, RK TI Longevity validation of the LOLA laser design by extended vacuum testing of the LOLA engineering model laser SO SOLID STATE LASERS XVIII: TECHNOLOGY AND DEVICES SE Proceedings of SPIE-The International Society for Optical Engineering LA English DT Proceedings Paper CT Conference on Solid State Lasers XVIII - Technology and Devices CY JAN 25-29, 2009 CL San Jose, CA SP SPIE, Coherent, Inc DE Lunar Orbiter Laser Altimeter; LOLA; Laser; Nd:YAG; Topography; LIDAR; Altimeter; Space laser ID MISSION AB The Lunar Orbiter Laser Altimeter (LOLA) is one of seven instruments aboard the Lunar Reconnaissance Orbiter (LRO) spacecraft with the objectives to determine the global topography of the lunar surface at high resolution, measure landing site slopes and search for polar ices in shadowed regions. The LOLA laser transmitter is a passively Q-switched crossed-Porro resonator. All components used in the laser have space flight heritage. The flight laser bench houses two oscillators (a primary and a cold spare) that are designed to operate sequentially during the mission. If the primary laser can no longer provide adequate scientific data products, the secondary laser will be turned on. The baseline mission calls for LOLA (and LRO) to spend about one year studying the Moon. Since LOLA operates at 28 Hz, the laser system needs to produce approximately one billion pulses during the primary one year mission. To validate that the LOLA laser design is capable of meeting this requirement, the LOLA Engineering Model (EM) laser has been subjected to extended operation testing in vacuum. In this paper we will summarize the longevity validation test effort of the LOLA EM laser. C1 [Shaw, George B.; Stephen, Mark A.; Troupaki, Elisavet; Vasilyev, Aleksey A.; Yu, Anthony W.] NASA, Goddard Space Flight Ctr, Laser & Electroopt Branch, Greenbelt, MD 20771 USA. RP Shaw, GB (reprint author), NASA, Goddard Space Flight Ctr, Laser & Electroopt Branch, MC554, Greenbelt, MD 20771 USA. NR 6 TC 2 Z9 2 U1 1 U2 2 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 978-0-8194-7439-1 J9 P SOC PHOTO-OPT INS PY 2009 VL 7193 AR 719306 DI 10.1117/12.814883 PG 12 WC Instruments & Instrumentation; Optics SC Instruments & Instrumentation; Optics GA BSL69 UT WOS:000284870500003 ER PT S AU Yu, AW Li, SX Shaw, GB Seas, A Stephen, MA Troupaki, E Vasilyev, A Ramos-Izquierdo, L Lukemier, A Mamakos, W Melak, A Guzek, J Rosanova, A AF Yu, Anthony W. Li, Steve X. Shaw, George B. Seas, Antonios Stephen, Mark A. Troupaki, Elisavet Vasilyev, Aleksey Ramos-Izquierdo, Luis Lukemier, Alan Mamakos, William Melak, Anthony Guzek, Jeff Rosanova, Alberto BE Clarkson, WA Hodgson, N Shori, RK TI Overview of Space Qualified Solid-State Lasers Development at NASA Goddard Space Flight Center SO SOLID STATE LASERS XVIII: TECHNOLOGY AND DEVICES SE Proceedings of SPIE-The International Society for Optical Engineering LA English DT Proceedings Paper CT Conference on Solid State Lasers XVIII - Technology and Devices CY JAN 25-29, 2009 CL San Jose, CA SP SPIE, Coherent, Inc DE Topography; LIDAR; Remote Sensing; Space Laser Systems; Laser Altimeter; Space-Qualified Lasers ID MESSENGER MISSION; MERCURY; ALTIMETER; TRANSMITTER; MARS AB NASA Goddard Space Flight Center (GSFC) has been engaging in Earth and planetary science instruments development for many years. With stunning topographic details of the Mars surface to Earth's surface maps and ice sheets dynamics of recent years, NASA GSFC has provided vast amount of scientific data products that gave detailed insights into Earth's and planetary sciences. In this paper we will review the past and present of space-qualified laser programs at GSFC and offer insights into future laser based science instrumentations. C1 [Yu, Anthony W.; Li, Steve X.; Shaw, George B.; Seas, Antonios; Stephen, Mark A.; Troupaki, Elisavet; Vasilyev, Aleksey; Ramos-Izquierdo, Luis; Lukemier, Alan; Mamakos, William; Melak, Anthony; Guzek, Jeff; Rosanova, Alberto] NASA, Goddard Space Flight Ctr, Laser & Electroopt Branch, Greenbelt, MD 20771 USA. RP Yu, AW (reprint author), NASA, Goddard Space Flight Ctr, Laser & Electroopt Branch, Greenbelt, MD 20771 USA. NR 28 TC 4 Z9 5 U1 1 U2 3 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 978-0-8194-7439-1 J9 P SOC PHOTO-OPT INS PY 2009 VL 7193 AR 719305 DI 10.1117/12.814954 PG 7 WC Instruments & Instrumentation; Optics SC Instruments & Instrumentation; Optics GA BSL69 UT WOS:000284870500002 ER PT S AU Loewenstein, M AF Loewenstein, Michael BE Cline, DB TI Suzaku search for evidence of sterile neutrinos in the Ursa Minor dwarf spheroidal galaxy SO SOURCES AND DETECTION OF DARK MATTER AND DARK ENERGY IN THE UNIVERSE SE AIP Conference Proceedings LA English DT Proceedings Paper CT 8th UCLA Symposium on Sources and Detection of Dark Matter and Dark Energy in the Universe CY FEB 20-22, 2008 CL Marina del Rey, CA SP Univ Calif Los Angeles DE sterile neutrinos; dark matter ID WARM DARK-MATTER; X-RAY; MILKY-WAY; OSCILLATIONS; SUPERNOVA; KICKS; XIS AB We present results of our search for X-ray line emission associated with the radiative decay of the sterile neutrino, a well-motivated dark matter candidate, in Suzaku Observatory spectra of the Ursa Minor dwarf spheroidal galaxy. These data represent the first deep observation of one of these extreme mass-to-light systems and the first dedicated dark matter search using an X-ray telescope. No such emission line is positively detected; and, we derive new upper limits that match or approach the best previous results over the entire 1-20 ke V mass range from a single Suzaku observation. These are used to place constraints on the existence of sterile neutrinos with given combinations of mass and active-sterile neutrino oscillation mixing angle in the general case, and in the case where they are assumed to constitute all of the dark matter. The allowed range implies that sterile neutrinos remain a viable candidate to make up some - or all - of the dark matter and also explain pulsar kicks and various other astrophysical phenomena. C1 [Loewenstein, Michael] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Loewenstein, M (reprint author), NASA, Goddard Space Flight Ctr, Code 662, Greenbelt, MD 20771 USA. NR 27 TC 0 Z9 0 U1 0 U2 0 PU AMER INST PHYSICS PI MELVILLE PA 2 HUNTINGTON QUADRANGLE, STE 1NO1, MELVILLE, NY 11747-4501 USA SN 0094-243X BN 978-0-7354-0703-9 J9 AIP CONF PROC PY 2009 VL 1166 BP 185 EP 190 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BPR82 UT WOS:000279741300025 ER PT S AU Abers, ES Bhatia, AK Dicus, DA Repko, WW Rosenbaum, DC Teplitz, VL AF Abers, E. S. Bhatia, A. K. Dicus, D. A. Repko, W. W. Rosenbaum, D. C. Teplitz, V. L. BE Cline, DB TI Strange Quark Nuggets in Space: Charges in Seven Settings SO SOURCES AND DETECTION OF DARK MATTER AND DARK ENERGY IN THE UNIVERSE SE AIP Conference Proceedings LA English DT Proceedings Paper CT 8th UCLA Symposium on Sources and Detection of Dark Matter and Dark Energy in the Universe CY FEB 20-22, 2008 CL Marina del Rey, CA SP Univ Calif Los Angeles ID NUCLEARITES; MATTER AB We have computed the charge that develops on an SQN in space as a result of balance between the rates of ionization by ambient gammas and capture of ambient electrons. We have also computed the tin-as for achieving that equilibrium and binding energy of the least bound SQN electrons. We have done this for seven different settings. We sketch the calculations here and give their results in the Figure and Table II; details are in the Physical Review D.79.023513 (2009). C1 [Abers, E. S.] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA. [Bhatia, A. K.; Teplitz, V. L.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Dicus, D. A.] Univ Texas Austin, Dept Phys, Austin, TX 78712 USA. [Repko, W. W.] Michigan State Univ, Dept Phys & Astron, E Lansing, MI 48824 USA. [Rosenbaum, D. C.; Teplitz, V. L.] Southern Methodist Univ, Dept Phys, Dallas, TX 75275 USA. RP Abers, ES (reprint author), Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA. FU U.S. Department of Energy [DE-FG03-93ER40757]; National Science Foundation [PHY-0555544] FX VLT very much appreciates a number of very helpful conversations with Demos Kazanas, one with Floyd Stecker on the diffuse gamma ray spectrum and one with M. Alford on effects of Cooper pairing. Dr. Alford kindly provided a number of insightful comments on the first version of this paper. DCR and VLT are also grateful to Jonathan Gardner for calling SN-2006gy to our attention, as well as C. Kilbourne for talking WHIM with us. DAD was supported in part by the U.S. Department of Energy under Grant No. DE-FG03-93ER40757. WWR was supported in part by the National Science Foundation under Grant PHY-0555544. NR 17 TC 0 Z9 0 U1 0 U2 0 PU AMER INST PHYSICS PI MELVILLE PA 2 HUNTINGTON QUADRANGLE, STE 1NO1, MELVILLE, NY 11747-4501 USA SN 0094-243X BN 978-0-7354-0703-9 J9 AIP CONF PROC PY 2009 VL 1166 BP 242 EP + PG 2 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BPR82 UT WOS:000279741300034 ER PT B AU Moltz, JC AF Moltz, James Clay BE Coletta, D Pilch, FT TI Russia and China Strategic choices in space SO SPACE AND DEFENSE POLICY SE Space Power and Politics LA English DT Article; Book Chapter C1 [Moltz, James Clay] NASA, Space Futures Working Grp, Ames Res Ctr, Washington, DC USA. [Moltz, James Clay] Monterey Inst Int Studies, CNS, Monterey, CA USA. NR 15 TC 0 Z9 0 U1 0 U2 0 PU ROUTLEDGE PI LONDON PA 11 NEW FETTER LANE, LONDON EC4P 4EE, ENGLAND BN 978-0-203-88306-8 J9 SPACE POWER POLIT PY 2009 BP 269 EP 289 PG 21 WC International Relations; Political Science SC International Relations; Government & Law GA BNL06 UT WOS:000274836500013 ER PT B AU Souza, KA Ilyin, EA Sychev, VN Jahns, GC AF Souza, Kenneth A. Ilyin, Eugene A. Sychev, Vladimir N. Jahns, Gary C. BE Sawin, CF Hanson, SI House, NG Pestov, ID TI Biological Research in Space SO SPACE BIOLOGY AND MEDICINE, VOL 5: U.S. AND RUSSIAN COOPERATION IN SPACE BIOLOGY AND MEDICINE SE Library of Flight LA English DT Article; Book Chapter ID MESSENGER-RNA LEVELS; ALTERED GRAVITATIONAL-FIELDS; PERIPHERAL-BLOOD LEUKOCYTES; LOCUS-COERULEUS NEURONS; BONE-MATRIX PROTEINS; LIFE-SUPPORT-SYSTEM; SKELETAL-MUSCLE; GENE-EXPRESSION; SPACEFLIGHT CONDITIONS; ESCHERICHIA-COLI C1 [Souza, Kenneth A.] NASA, Ames Res Ctr, Mail Code SC, Mountain View, CA 94035 USA. [Ilyin, Eugene A.; Sychev, Vladimir N.] Inst Biomed Problems, State Res Ctr, Moscow 123007, Russia. [Jahns, Gary C.] NASA, Ames Res Ctr, Mail Code VB, Mountain View, CA 94035 USA. RP Souza, KA (reprint author), NASA, Ames Res Ctr, Mail Code SC, Mountain View, CA 94035 USA. EM Kenneth.A.Souza@nasa.gov; ilyine@imbp.ru; Gary.c.jahns@nasa.gov NR 291 TC 1 Z9 1 U1 0 U2 1 PU AMER INST AERONAUTICS & ASTRONAUTICS PI RESTON PA 1801 ALEXANDER BELL DR, STE 500, RESTON, VA 20191-4344 USA BN 978-1-56347-996-0 J9 LIBR FLIGHT PY 2009 BP 1 EP 43 PG 43 WC Engineering, Aerospace; Biology; Medicine, Research & Experimental SC Engineering; Life Sciences & Biomedicine - Other Topics; Research & Experimental Medicine GA BKU32 UT WOS:000269263900002 ER PT B AU House, NG Samarin, GI AF House, Nancy G. Samarin, G. I. BE Sawin, CF Hanson, SI House, NG Pestov, ID TI Biomedical Research in Spaceflight SO SPACE BIOLOGY AND MEDICINE, VOL 5: U.S. AND RUSSIAN COOPERATION IN SPACE BIOLOGY AND MEDICINE SE Library of Flight LA English DT Article; Book Chapter ID INTERNATIONAL-SPACE-STATION; ORTHOSTATIC HYPOTENSION; BONE METABOLISM; ASTRONAUTS; FLIGHT C1 [House, Nancy G.] NASA, Lyndon B Johnson Space Ctr, Stinger Ghaffarian Technol Mail Code ZB, Houston, TX 77058 USA. [Samarin, G. I.] Inst Biomed Problems, State Res Ctr, Moscow 123007, Russia. RP House, NG (reprint author), NASA, Lyndon B Johnson Space Ctr, Stinger Ghaffarian Technol Mail Code ZB, Houston, TX 77058 USA. EM Nancy.g.house@nasa.gov; samarin@imbp.ru; Nancy.g.house@nasa.gov NR 36 TC 1 Z9 1 U1 0 U2 0 PU AMER INST AERONAUTICS & ASTRONAUTICS PI RESTON PA 1801 ALEXANDER BELL DR, STE 500, RESTON, VA 20191-4344 USA BN 978-1-56347-996-0 J9 LIBR FLIGHT PY 2009 BP 69 EP 194 PG 126 WC Engineering, Aerospace; Biology; Medicine, Research & Experimental SC Engineering; Life Sciences & Biomedicine - Other Topics; Research & Experimental Medicine GA BKU32 UT WOS:000269263900004 ER PT B AU Katuntsev, VP Osipov, YY Gernhardt, M Dervay, J Thomas, KS Reeves, JM AF Katuntsev, V. P. Osipov, Yu Yu. Gernhardt, M. Dervay, J. Thomas, K. S. Reeves, J. M. BE Sawin, CF Hanson, SI House, NG Pestov, ID TI Extravehicular Activity SO SPACE BIOLOGY AND MEDICINE, VOL 5: U.S. AND RUSSIAN COOPERATION IN SPACE BIOLOGY AND MEDICINE SE Library of Flight LA English DT Article; Book Chapter ID DECOMPRESSION-SICKNESS; ALTITUDE DECOMPRESSION; EVA; PRESSURE; SUPPORT; MIR C1 [Katuntsev, V. P.; Osipov, Yu Yu.] Inst Biomed Problems, State Res Ctr, Moscow 123007, Russia. [Gernhardt, M.] NASA, Lyndon B Johnson Space Ctr, Mail Code CB, Houston, TX 77058 USA. [Thomas, K. S.] Hamilton Sundstrand Corp, Windsor Locks, CT 06096 USA. [Dervay, J.] NASA, Lyndon B Johnson Space Ctr, Mail Code SD2, Houston, TX 77058 USA. [Reeves, J. M.] NASA, Lyndon B Johnson Space Ctr, Muniz Engn Inc, Mail Code SK, Houston, TX 77058 USA. RP Katuntsev, VP (reprint author), Inst Biomed Problems, State Res Ctr, 76A Khoroshevskoye Shosse, Moscow 123007, Russia. EM katuntsev@imbp.ru; osipov@imbp.ru; michael.l.gernhardt@nasa.gov; joseph.p.dervay@nasa.gov; jacqueline.m.reeves@nasa.gov NR 47 TC 0 Z9 0 U1 0 U2 0 PU AMER INST AERONAUTICS & ASTRONAUTICS PI RESTON PA 1801 ALEXANDER BELL DR, STE 500, RESTON, VA 20191-4344 USA BN 978-1-56347-996-0 J9 LIBR FLIGHT PY 2009 BP 195 EP 233 PG 39 WC Engineering, Aerospace; Biology; Medicine, Research & Experimental SC Engineering; Life Sciences & Biomedicine - Other Topics; Research & Experimental Medicine GA BKU32 UT WOS:000269263900005 ER PT B AU Baranov, VM Mccoy, JT Agureev, AN AF Baranov, V. M. McCoy, J. Torin Agureev, Aleksandr N. BE Sawin, CF Hanson, SI House, NG Pestov, ID TI Habitable Environment of the International Space Station Overview SO SPACE BIOLOGY AND MEDICINE, VOL 5: U.S. AND RUSSIAN COOPERATION IN SPACE BIOLOGY AND MEDICINE SE Library of Flight LA English DT Editorial Material; Book Chapter C1 [Baranov, V. M.; Agureev, Aleksandr N.] Russian Acad Sci, State Res Ctr, Inst Biomed Problems, Moscow 123007, Russia. [McCoy, J. Torin] NASA, Lyndon B Johnson Space Ctr, Environm Factors Branch, Space & Life Sci Directorate, Washington, DC USA. RP Baranov, VM (reprint author), Russian Acad Sci, State Res Ctr, Inst Biomed Problems, 76A Khoroshevskoye Shosse, Moscow 123007, Russia. EM baranov@imbp.ru; aagureev@imbp.ru NR 0 TC 0 Z9 0 U1 0 U2 0 PU AMER INST AERONAUTICS & ASTRONAUTICS PI RESTON PA 1801 ALEXANDER BELL DR, STE 500, RESTON, VA 20191-4344 USA BN 978-1-56347-996-0 J9 LIBR FLIGHT PY 2009 BP 235 EP 236 PG 2 WC Engineering, Aerospace; Biology; Medicine, Research & Experimental SC Engineering; Life Sciences & Biomedicine - Other Topics; Research & Experimental Medicine GA BKU32 UT WOS:000269263900006 ER PT B AU Bogatova, RI Allen, CS Kutina, IV Goodman, JR AF Bogatova, R. I. Allen, C. S. Kutina, I. V. Goodman, J. R. BE Sawin, CF Hanson, SI House, NG Pestov, ID TI Microclimate, Acoustic Environment, and Lighting Conditions SO SPACE BIOLOGY AND MEDICINE, VOL 5: U.S. AND RUSSIAN COOPERATION IN SPACE BIOLOGY AND MEDICINE SE Library of Flight LA English DT Article; Book Chapter C1 [Bogatova, R. I.; Kutina, I. V.] Inst Biomed Problems, State Res Ctr, Moscow 123007, Russia. [Allen, C. S.; Goodman, J. R.] NASA, Lyndon B Johnson Space Ctr, Mail Code SF2, Houston, TX 77058 USA. RP Bogatova, RI (reprint author), Inst Biomed Problems, State Res Ctr, 76A Khoroshevskoye Shosse, Moscow 123007, Russia. EM rimma@imbp.ru; christopher.s.allen@nasa.gov; jerry.r.goodman@nasa.gov NR 30 TC 0 Z9 0 U1 0 U2 0 PU AMER INST AERONAUTICS & ASTRONAUTICS PI RESTON PA 1801 ALEXANDER BELL DR, STE 500, RESTON, VA 20191-4344 USA BN 978-1-56347-996-0 J9 LIBR FLIGHT PY 2009 BP 237 EP 248 PG 12 WC Engineering, Aerospace; Biology; Medicine, Research & Experimental SC Engineering; Life Sciences & Biomedicine - Other Topics; Research & Experimental Medicine GA BKU32 UT WOS:000269263900007 ER PT B AU Mukhamedieva, LN James, JT Aksel-Rubinstein, VZ Solomin, GI AF Mukhamedieva, L. N. James, J. T. Aksel-Rubinstein, V. Z. Solomin, G. I. BE Sawin, CF Hanson, SI House, NG Pestov, ID TI Toxicology of the International Space Station Atmosphere SO SPACE BIOLOGY AND MEDICINE, VOL 5: U.S. AND RUSSIAN COOPERATION IN SPACE BIOLOGY AND MEDICINE SE Library of Flight LA English DT Article; Book Chapter C1 [Mukhamedieva, L. N.; Solomin, G. I.] Inst Biomed Problems, State Res Ctr, Moscow 123007, Russia. [Aksel-Rubinstein, V. Z.] Minist Hlth Russian Federat, GUP Sci Res Inst Ind & Marine Med, St Petersburg 196143, Russia. [James, J. T.] NASA, Lyndon B Johnson Space Ctr, Mail Code SF, Houston, TX 77058 USA. RP Mukhamedieva, LN (reprint author), Inst Biomed Problems, State Res Ctr, 76A Khoroshevskoye Shosse, Moscow 123007, Russia. EM moukhamedieva@imbp.ru; john.t.james@nasa.gov NR 23 TC 0 Z9 0 U1 0 U2 0 PU AMER INST AERONAUTICS & ASTRONAUTICS PI RESTON PA 1801 ALEXANDER BELL DR, STE 500, RESTON, VA 20191-4344 USA BN 978-1-56347-996-0 J9 LIBR FLIGHT PY 2009 BP 249 EP 262 PG 14 WC Engineering, Aerospace; Biology; Medicine, Research & Experimental SC Engineering; Life Sciences & Biomedicine - Other Topics; Research & Experimental Medicine GA BKU32 UT WOS:000269263900008 ER PT B AU Novikova, ND Pierson, DL Poddubko, SV Deshevaya, YA Ott, CM Castro, VA Bruce, RJ AF Novikova, N. D. Pierson, D. L. Poddubko, S. V. Deshevaya, Ye. A. Ott, C. M. Castro, V. A. Bruce, R. J. BE Sawin, CF Hanson, SI House, NG Pestov, ID TI Microbiology of the International Space Station SO SPACE BIOLOGY AND MEDICINE, VOL 5: U.S. AND RUSSIAN COOPERATION IN SPACE BIOLOGY AND MEDICINE SE Library of Flight LA English DT Article; Book Chapter ID ASTRONAUTS; SPACEFLIGHT; REACTIVATION; BACTERIA; SYSTEM C1 [Novikova, N. D.; Poddubko, S. V.; Deshevaya, Ye. A.] Inst Biomed Problems, State Res Ctr, Moscow 123007, Russia. [Bruce, R. J.] NASA, Lyndon B Johnson Space Ctr, Enterprise Advisory Serv Inc, Mail Code SF, Houston, TX 77058 USA. [Pierson, D. L.] NASA, Lyndon B Johnson Space Ctr, Mail Code SF2, Houston, TX 77058 USA. RP Novikova, ND (reprint author), Inst Biomed Problems, State Res Ctr, 76A Khoroshevskoye Shosse, Moscow 123007, Russia. EM novikova@imbp.ru; duane.l.pierson@nasa.gov; poddubko@imbp.ru; charlie.m.ott@nasa.gov; victoria.a.castro@nasa.gov; rebekah.j.bruce@nasa.gov NR 51 TC 0 Z9 0 U1 3 U2 6 PU AMER INST AERONAUTICS & ASTRONAUTICS PI RESTON PA 1801 ALEXANDER BELL DR, STE 500, RESTON, VA 20191-4344 USA BN 978-1-56347-996-0 J9 LIBR FLIGHT PY 2009 BP 263 EP 278 PG 16 WC Engineering, Aerospace; Biology; Medicine, Research & Experimental SC Engineering; Life Sciences & Biomedicine - Other Topics; Research & Experimental Medicine GA BKU32 UT WOS:000269263900009 ER PT B AU Petrov, VA Cucinotta, FA AF Petrov, V. A. Cucinotta, F. A. BE Sawin, CF Hanson, SI House, NG Pestov, ID TI Radiation Safety of International Space Station Crews SO SPACE BIOLOGY AND MEDICINE, VOL 5: U.S. AND RUSSIAN COOPERATION IN SPACE BIOLOGY AND MEDICINE SE Library of Flight LA English DT Article; Book Chapter ID GALACTIC COSMIC-RAYS; CHROMOSOME-ABERRATIONS; BLOOD-LYMPHOCYTES; CANCER; PROTECTION; ASTRONAUTS; EQUIVALENT; DEPENDENCE; SPECTRA; RISK C1 [Petrov, V. A.] Inst Biomed Problems, State Res Ctr, Moscow 123007, Russia. [Cucinotta, F. A.] NASA, Lyndon B Johnson Space Ctr, Mail Code SK, Houston, TX 77058 USA. RP Petrov, VA (reprint author), Inst Biomed Problems, State Res Ctr, 76A Khoroshevskoye Shosse, Moscow 123007, Russia. EM petrov@pike.net.ru; francis.a.cucinotta@nasa.gov NR 44 TC 0 Z9 0 U1 0 U2 0 PU AMER INST AERONAUTICS & ASTRONAUTICS PI RESTON PA 1801 ALEXANDER BELL DR, STE 500, RESTON, VA 20191-4344 USA BN 978-1-56347-996-0 J9 LIBR FLIGHT PY 2009 BP 279 EP 299 PG 21 WC Engineering, Aerospace; Biology; Medicine, Research & Experimental SC Engineering; Life Sciences & Biomedicine - Other Topics; Research & Experimental Medicine GA BKU32 UT WOS:000269263900010 ER PT B AU Skuratov, VM Mudgett, PD Bobe, LS Andreichuk, PO Schultz, JR AF Skuratov, V. M. Mudgett, P. D. Bobe, L. S. Andreichuk, P. O. Schultz, J. R. BE Sawin, CF Hanson, SI House, NG Pestov, ID TI Water Supply on the International Space Station Station Water Supply System and Operating Results November 2, 2000-April 20, 2007 (Increments ISS-1-ISS-14) SO SPACE BIOLOGY AND MEDICINE, VOL 5: U.S. AND RUSSIAN COOPERATION IN SPACE BIOLOGY AND MEDICINE SE Library of Flight LA English DT Article; Book Chapter C1 [Skuratov, V. M.] Inst Biomed Problems, State Res Ctr, Moscow 123007, Russia. [Bobe, L. S.] OAO Sci Res Inst KhimMash, Moscow 127015, Russia. [Andreichuk, P. O.] Energiya Rocket Space Corp, Sci Prod Org, Korolev 141070, Moscovskaya Obl, Russia. [Mudgett, P. D.] NASA, Lyndon B Johnson Space Ctr, Mail Code SF2, Houston, TX 77058 USA. [Schultz, J. R.] NASA, Lyndon B Johnson Space Ctr, Mail Code SF, Houston, TX 77058 USA. RP Skuratov, VM (reprint author), Inst Biomed Problems, State Res Ctr, 76A Khoroshevskoye Shosse, Moscow 123007, Russia. EM paul.d.mudgett@nasa.gov; l_bobe@niichimmash.ru; john.r.schultz@nasa.gov NR 16 TC 0 Z9 0 U1 1 U2 1 PU AMER INST AERONAUTICS & ASTRONAUTICS PI RESTON PA 1801 ALEXANDER BELL DR, STE 500, RESTON, VA 20191-4344 USA BN 978-1-56347-996-0 J9 LIBR FLIGHT PY 2009 BP 301 EP 311 PG 11 WC Engineering, Aerospace; Biology; Medicine, Research & Experimental SC Engineering; Life Sciences & Biomedicine - Other Topics; Research & Experimental Medicine GA BKU32 UT WOS:000269263900011 ER PT B AU Agureev, AN Kloeris, V Zwart, SR Smith, SM AF Agureev, A. N. Kloeris, V. Zwart, S. R. Smith, S. M. BE Sawin, CF Hanson, SI House, NG Pestov, ID TI Nutrition for International Space Station Crews SO SPACE BIOLOGY AND MEDICINE, VOL 5: U.S. AND RUSSIAN COOPERATION IN SPACE BIOLOGY AND MEDICINE SE Library of Flight LA English DT Article; Book Chapter ID VITAMIN-K; FLIGHT; ASTRONAUTS; METABOLISM; MARKERS C1 [Agureev, A. N.] Inst Biomed Problems, State Res Ctr, Moscow 123007, Russia. [Kloeris, V.] NASA, Lyndon B Johnson Space Ctr, Mail Code SF3, Houston, TX 77058 USA. [Smith, S. M.] NASA, Lyndon B Johnson Space Ctr, Mail Code SK3, Houston, TX 77058 USA. [Zwart, S. R.] NASA, Lyndon B Johnson Space Ctr, Univ Space Res Assoc, Mail Code SK, Houston, TX 77058 USA. RP Agureev, AN (reprint author), Inst Biomed Problems, State Res Ctr, 76A Khoroshevskoye Shosse, Moscow 123007, Russia. EM aagureev@imbp.ru; vickie.l.kloeris@nasa.gov; sara.zwart-1@nasa.gov; scott.m.smith@nasa.gov NR 44 TC 0 Z9 0 U1 0 U2 1 PU AMER INST AERONAUTICS & ASTRONAUTICS PI RESTON PA 1801 ALEXANDER BELL DR, STE 500, RESTON, VA 20191-4344 USA BN 978-1-56347-996-0 J9 LIBR FLIGHT PY 2009 BP 313 EP 324 PG 12 WC Engineering, Aerospace; Biology; Medicine, Research & Experimental SC Engineering; Life Sciences & Biomedicine - Other Topics; Research & Experimental Medicine GA BKU32 UT WOS:000269263900012 ER PT B AU Shumilina, GA Villarreal, JD AF Shumilina, G. A. Villarreal, J. D. BE Sawin, CF Hanson, SI House, NG Pestov, ID TI Personal Hygiene for International Space Station Crewmembers SO SPACE BIOLOGY AND MEDICINE, VOL 5: U.S. AND RUSSIAN COOPERATION IN SPACE BIOLOGY AND MEDICINE SE Library of Flight LA English DT Article; Book Chapter C1 [Villarreal, J. D.] NASA, Lyndon B Johnson Space Ctr, Mail Code EC1, Houston, TX 77058 USA. EM jennifer.d.villarreal@nasa.gov NR 20 TC 0 Z9 0 U1 0 U2 0 PU AMER INST AERONAUTICS & ASTRONAUTICS PI RESTON PA 1801 ALEXANDER BELL DR, STE 500, RESTON, VA 20191-4344 USA BN 978-1-56347-996-0 J9 LIBR FLIGHT PY 2009 BP 325 EP 330 PG 6 WC Engineering, Aerospace; Biology; Medicine, Research & Experimental SC Engineering; Life Sciences & Biomedicine - Other Topics; Research & Experimental Medicine GA BKU32 UT WOS:000269263900013 ER PT B AU Bogomolov, VV Duncan, JM Sargsyan, AE Pool, SL AF Bogomolov, V. V. Duncan, J. M. Sargsyan, A. E. Pool, S. L. BE Sawin, CF Hanson, SI House, NG Pestov, ID TI Medical Support for Crewmembers of the International Space Station SO SPACE BIOLOGY AND MEDICINE, VOL 5: U.S. AND RUSSIAN COOPERATION IN SPACE BIOLOGY AND MEDICINE SE Library of Flight LA English DT Article; Book Chapter ID MIR; FLIGHT; SPACEFLIGHT; LONG; QUALIFICATION; MICROGRAVITY; SHUTTLE/MIR; EXPERIENCES; PROGRAM; HEALTH C1 [Bogomolov, V. V.] Inst Biomed Problems, State Res Ctr, Moscow 123007, Russia. [Duncan, J. M.] NASA, Lyndon B Johnson Space Ctr, Mail Code SD, Houston, TX 77058 USA. [Sargsyan, A. E.] NASA, Lyndon B Johnson Space Ctr, Mail Code SD2, Houston, TX 77058 USA. RP Bogomolov, VV (reprint author), Inst Biomed Problems, State Res Ctr, 76A Khoroshevskoye Shosse, Moscow 123007, Russia. EM vvb@imbp.ru; james.m.duncan@nasa.gov; ashot.sargsyan-1@nasa.gov; SLPool@earthlink.net NR 59 TC 0 Z9 0 U1 0 U2 0 PU AMER INST AERONAUTICS & ASTRONAUTICS PI RESTON PA 1801 ALEXANDER BELL DR, STE 500, RESTON, VA 20191-4344 USA BN 978-1-56347-996-0 J9 LIBR FLIGHT PY 2009 BP 331 EP 394 PG 64 WC Engineering, Aerospace; Biology; Medicine, Research & Experimental SC Engineering; Life Sciences & Biomedicine - Other Topics; Research & Experimental Medicine GA BKU32 UT WOS:000269263900014 ER PT B AU Grigoriev, AI Potapov, AN Jones, JA Sullivan, TA Scheuring, RA AF Grigoriev, A. I. Potapov, A. N. Jones, J. A. Sullivan, T. A. Scheuring, R. A. BE Sawin, CF Hanson, SI House, NG Pestov, ID TI Medical Support for Interplanetary Human Spaceflights SO SPACE BIOLOGY AND MEDICINE, VOL 5: U.S. AND RUSSIAN COOPERATION IN SPACE BIOLOGY AND MEDICINE SE Library of Flight LA English DT Article; Book Chapter ID INTERNATIONAL-SPACE-STATION; LONG-DURATION SPACEFLIGHT; MICROGRAVITY; ASTRONAUTS; MISSION; RISK; COUNTERMEASURE; PARTICLES; RADIATION; ABOARD C1 [Grigoriev, A. I.; Potapov, A. N.] Inst Biomed Problems, State Res Ctr, Moscow 123007, Russia. [Jones, J. A.] NASA, Lyndon B Johnson Space Ctr, Mail Code SD2, Houston, TX 77058 USA. [Sullivan, T. A.] NASA, Lyndon B Johnson Space Ctr, Mail Code SF, Houston, TX 77058 USA. [Scheuring, R. A.] NASA, Lyndon B Johnson Space Ctr, Mail Code SD, Houston, TX 77058 USA. RP Grigoriev, AI (reprint author), Inst Biomed Problems, State Res Ctr, 76A Khoroshevskoye Shosse, Moscow 123007, Russia. EM grigoriev@imbp.ru; potapov@imbp.ru; jeffrey.a.jones@nasa.gov; thomas.a.suilivan@nasa.gov; richard.a.scheuring@nasa.gov NR 167 TC 2 Z9 2 U1 0 U2 0 PU AMER INST AERONAUTICS & ASTRONAUTICS PI RESTON PA 1801 ALEXANDER BELL DR, STE 500, RESTON, VA 20191-4344 USA BN 978-1-56347-996-0 J9 LIBR FLIGHT PY 2009 BP 395 EP 454 PG 60 WC Engineering, Aerospace; Biology; Medicine, Research & Experimental SC Engineering; Life Sciences & Biomedicine - Other Topics; Research & Experimental Medicine GA BKU32 UT WOS:000269263900015 ER PT B AU Jones, SM AF Jones, Steven M. BE Denis, JH Aldridge, PD TI SPACE SCIENCE APPLICATIONS OF AEROGELS SO SPACE EXPLORATION RESEARCH SE Space Science Exploration and Policy LA English DT Article; Book Chapter ID SOL-GEL PROCESS; SILICA AEROGEL; COMET 81P/WILD-2; IMPACT FEATURES; STARDUST; DUST; IDENTIFICATION; CHEMISTRY AB The unique physical properties of aerogels have provided enabling technologies to a variety of both flight and proposed space science missions. The extremely low values of the density and corresponding high values of the porosity of aerogels make them suitable for stopping high velocity particles, as highly efficient thermal barriers and as a porous medium for the containment of cryogenic fluids. The use of silica aerogel as a hypervelocity particle capture and return medium for the Stardust Mission, which launched in 1999 and returned to earth in 2006, has drawn the attention of the scientific community, as well as the public, to these fascinating materials. Aerogels are currently being used as the thermal insulation material in the 2003 Mars Exploration Rovers and will be used on the 2009 Mars Science Laboratory rover, as well. The SCIM (Sample Collection for the Investigation of Mars) and the STEP (Satellite Test of the Equivalence Principle) Missions are proposed scientific missions, in which the use of aerogel is critical to their overall design and success. Composite materials comprised of silica aerogel and oxide powders are currently under development for use in a new generation of thermoelectric devices that are planned for use in future mission designs. Work is ongoing in the development and production of non-silicate and composite aerogels to extend the range of useful physical properties, and thus, the applications of aerogels in future space science missions. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. RP Jones, SM (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. EM Steven.M.Jones@jpl.nasa.gov NR 43 TC 0 Z9 0 U1 0 U2 0 PU NOVA SCIENCE PUBLISHERS, INC PI HAUPPAUGE PA 400 OSER AVE, STE 1600, HAUPPAUGE, NY 11788-3635 USA BN 978-1-60692-264-4 J9 SPACE SCI EXPLOR POL PY 2009 BP 361 EP 384 PG 24 WC Engineering, Aerospace; Astronomy & Astrophysics SC Engineering; Astronomy & Astrophysics GA BNV31 UT WOS:000275662600014 ER PT S AU Bugby, D Seghi, S Kroliczek, E Pauken, M AF Bugby, D. Seghi, S. Kroliczek, E. Pauken, M. BE Robertson, GA TI Novel Architecture for a Long-Life, Lightweight Venus Lander SO SPACE, PROPULSION & ENERGY SCIENCES INTERNATIONAL FORUM SPESIF-2009 SE AIP Conference Proceedings LA English DT Proceedings Paper CT 13th Conference on Thermophysics Applications in Microgravity/6th Symposium on New Frontiers in Space Propulsion Sciences/1st Symposium on Astrosociology CY FEB 24-26, 2009 CL Huntsville, AL SP Amer Astronaut Soc, Amer Inst Aeronaut & Astronaut, Astrosociol Res Inst DE Spacecraft; Venus; Lander; Long-Life; Lightweight; Thermal; Architecture; Evaporation; Water; Insulation AB This paper describes a novel concept for an extended lifetime, lightweight Venus lander. Historically, to operate in the 480 degrees C, 90 atm, corrosive, mostly CO2 Venus surface environment, previous landers have relied on thick Ti spherical outer shells and thick layers of internal insulation. But even the most resilient of these landers operated for only about 2 hours before succumbing to the environment. The goal on this project is to develop an architecture that extends lander lifetime to 20-25 hours and also reduces mass compared to the Pioneer Venus mission architecture. The idea for reducing mass is to: (a) contain the science instruments within a spherical high strength lightweight polymer matrix composite (PMC) tank; (b) surround the PMC tank with an annular shell of high performance insulation pre-pressurized to a level that (after landing) will exceed the external Venus surface pressure; and (c) surround the insulation with a thin Ti outer shell that contains only a net internal pressure, eliminating buckling overdesign mass. The combination of the PMC inner tank and thin Ti outer shell is lighter than a single thick Ti outer shell. The idea for extending lifetime is to add the following three features: (i) an expendable water supply that is placed within the insulation or is contained in an additional vessel within the PMC tank; (ii) a thin spherical evaporator shell placed within the insulation a short radial distance from the outer shell; and (iii) a thin heat-intercepting liquid cooled shield placed inboard of the evaporator shell. These features lower the temperature of the insulation below what it would have been with the insulation alone, reducing the internal heat leak and lengthening lifetime. The use of phase change materials (PCMs) inside the PMC tank is also analyzed as a lifetime-extending design option. The paper describes: (1) analytical modeling to demonstrate reduced mass and extended life; (2) thermal conductivity testing of high performance insulation as a function of temperature and pressure; (3) a bench-top ambient pressure thermal test of the evaporation system; and (4) a higher fidelity test, to be conducted in a high pressure, high temperature inert gas test chamber, of a small-scale Venus lander prototype (made from two hemispherical interconnecting halves) that includes all of the aforesaid features. 22 CFR 125.4(b)(13) applicable C1 [Bugby, D.] ATK Space, 5050 Powder Mill Rd, Beltsville, MD 20705 USA. [Seghi, S.] Ceram Compos Inc, Annapolis, MD 21401 USA. [Kroliczek, E.] B & K Engn, Davidsonville, MD USA. [Pauken, M.] Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. RP Bugby, D (reprint author), ATK Space, 5050 Powder Mill Rd, Beltsville, MD 20705 USA. EM david.bugby@atk.com NR 1 TC 0 Z9 0 U1 0 U2 0 PU AMER INST PHYSICS PI MELVILLE PA 2 HUNTINGTON QUADRANGLE, STE 1NO1, MELVILLE, NY 11747-4501 USA SN 0094-243X BN 978-0-7354-0639-1 J9 AIP CONF PROC PY 2009 VL 1103 BP 39 EP 50 PG 12 WC Engineering, Aerospace; Astronomy & Astrophysics; Energy & Fuels SC Engineering; Astronomy & Astrophysics; Energy & Fuels GA BJG15 UT WOS:000265592900005 ER PT S AU Williams, GJ Gilland, JH AF Williams, George J., Jr. Gilland, James H. BE Robertson, GA TI Propulsion Utilizing Laser-Driven Ponderomotive Fields for Deep-Space Missions SO SPACE, PROPULSION & ENERGY SCIENCES INTERNATIONAL FORUM SPESIF-2009 SE AIP Conference Proceedings LA English DT Proceedings Paper CT 13th Conference on Thermophysics Applications in Microgravity/6th Symposium on New Frontiers in Space Propulsion Sciences/1st Symposium on Astrosociology CY FEB 24-26, 2009 CL Huntsville, AL SP Amer Astronaut Soc, Amer Inst Aeronaut & Astronaut, Astrosociol Res Inst DE Laser Propulsion; Ponderomotive; Interstellar Propulsion AB The generation of large amplitude electric fields in plasmas by high-power lasers has been studied for several years in the context of high-energy particle acceleration. Fields on the order of GeV/m are generated in the plasma wake of the laser by non-linear ponderomotive forces. The laser fields generate longitudinal and translational electron plasma waves with phase velocities close to the speed of light. These fields and velocities offer the potential to revolutionize spacecraft propulsion, leading to extended deep space robotic probes. Based on these initial calculations, plasma acceleration by means of laser-induced ponderomotive forces appears to offer significant potential for spacecraft propulsion. Relatively high-efficiencies appear possible with proper beam conditioning, resulting in an order of magnitude more thrust than alternative concepts for high I(sp) (>10(5) s) and elimination of the primary life-limiting erosion phenomena associated with conventional electric propulsion systems. Ponderomotive propulsion readily lends itself to beamed power which might overcome some of the constraints of power-limited propulsion concepts. A preliminary assessment of the impact of these propulsion systems for several promising configurations on mission architectures has been conducted. Emphasizing interstellar and interstellar-precursor applications, performance and technical requirements are identified for a number of missions. The use of in-situ plasma and gas for propellant is evaluated as well. C1 [Williams, George J., Jr.; Gilland, James H.] NASA, Ohio Aerosp Inst, GRCMS 16 1, Cleveland, OH 44135 USA. RP Williams, GJ (reprint author), NASA, Ohio Aerosp Inst, GRCMS 16 1, Cleveland, OH 44135 USA. EM George.J.Williams@nasa.gov; James.H.Gilland@nasa.gov NR 22 TC 0 Z9 0 U1 0 U2 1 PU AMER INST PHYSICS PI MELVILLE PA 2 HUNTINGTON QUADRANGLE, STE 1NO1, MELVILLE, NY 11747-4501 USA SN 0094-243X BN 978-0-7354-0639-1 J9 AIP CONF PROC PY 2009 VL 1103 BP 175 EP 184 PG 10 WC Engineering, Aerospace; Astronomy & Astrophysics; Energy & Fuels SC Engineering; Astronomy & Astrophysics; Energy & Fuels GA BJG15 UT WOS:000265592900021 ER PT S AU Swanson, TD AF Swanson, Theodore D. BE Robertson, GA TI Space Exploration and the Greenland Norse; A Comparative Study on the Application of Technology for Exploration SO SPACE, PROPULSION & ENERGY SCIENCES INTERNATIONAL FORUM SPESIF-2009 SE AIP Conference Proceedings LA English DT Proceedings Paper CT 13th Conference on Thermophysics Applications in Microgravity/6th Symposium on New Frontiers in Space Propulsion Sciences/1st Symposium on Astrosociology CY FEB 24-26, 2009 CL Huntsville, AL SP Amer Astronaut Soc, Amer Inst Aeronaut & Astronaut, Astrosociol Res Inst DE Exploration; Space; Greenland Norse; Technology; Survival AB During the mid to late Middle Ages a group of intrepid explorers from Scandinavia established two colonies in the harsh environment of Greenland. These people were known as the Greenland Norse. While their colonies made a determined effort and survived for about 500 years, they never really flourished and struggled just to survive in their harsh environment. Eventually they disappeared, despite the fact that a neighboring group, the Inuits, was successful in surviving into the modem era. Hence, while survival was very difficult due to a variety of factors, it was possible depending on how the society dealt with the environment. There are a number of interesting parallels between this Greenland Norse experiment and the modem era of space exploration. While comparisons from the past to present day plans must certainly be made with caution, there may be interesting lessons to learn. Specifically, the role of technology and innovation by the Greenland Norse is addressed in this comparative study. C1 NASA, Goddard Space Flight Ctr, Washington, DC 20546 USA. RP Swanson, TD (reprint author), NASA, Goddard Space Flight Ctr, Washington, DC 20546 USA. EM Theodore.D.Swanson@nasa.gov NR 10 TC 0 Z9 0 U1 0 U2 0 PU AMER INST PHYSICS PI MELVILLE PA 2 HUNTINGTON QUADRANGLE, STE 1NO1, MELVILLE, NY 11747-4501 USA SN 0094-243X BN 978-0-7354-0639-1 J9 AIP CONF PROC PY 2009 VL 1103 BP 407 EP 413 PG 7 WC Engineering, Aerospace; Astronomy & Astrophysics; Energy & Fuels SC Engineering; Astronomy & Astrophysics; Energy & Fuels GA BJG15 UT WOS:000265592900049 ER PT S AU Clark, PE Millar, PS Beaman, B Choi, M Cooper, L Feng, S King, R Leshin, L Lewis, R Yeh, PS Young, E Lorenz, J AF Clark, P. E. Millar, P. S. Beaman, B. Choi, M. Cooper, L. Feng, S. King, R. Leshin, L. Lewis, R. Yeh, P. S. Young, E. Lorenz, J. BE Robertson, GA TI Enabling Technology for Lunar Surface Science SO SPACE, PROPULSION & ENERGY SCIENCES INTERNATIONAL FORUM SPESIF-2009 SE AIP Conference Proceedings LA English DT Proceedings Paper CT 13th Conference on Thermophysics Applications in Microgravity/6th Symposium on New Frontiers in Space Propulsion Sciences/1st Symposium on Astrosociology CY FEB 24-26, 2009 CL Huntsville, AL SP Amer Astronaut Soc, Amer Inst Aeronaut & Astronaut, Astrosociol Res Inst DE Moon; Lunar Surface; Instrumentation; Space Physics; Space Environment; Space Radiation; Atmosphere; Magnetic Field; Plasma; Dust; Geophysics; Interior; Heat Flow; Seismometry; Astrophysics AB Implementation of Lunar Exploration Initiative goals will require deployment of science packages at sites with the appropriate vantage point for obtaining the desired measurements and remote from potential (human) sources of contamination, thus requiring stand alone operation. Chief instruments/instrument package candidates include those which could provide long-term monitoring of the surface and subsurface environments for fundamental lunar science and crew safety. The major challenge such packages face will be operating during long periods of darkness in extreme cold potentially without the Pu238 based power and thermal systems available to Apollo era packages (ALSEP). The initial attempt to design a 10 instrument environmental monitoring package with a solar/battery based power system led to a package with a unacceptably large mass (500 kg) of which over half was battery mass. We achieved considerable reduction in this mass, first through the introduction of high performance electronics capable of operating at far lower temperature, reducing the initial mass estimate by a factor of 2, and then through the use of innovative thermal balance strategies involving the use of multi-layer thin materials and gravity-assisted heat pipes, reducing the initial mass estimate by a factor of 5. Yet to be implemented are strategies involving the universal incorporation of ULT/ULP (Ultra Low Temperature/Ultra Low Power) digital and analog electronics, distributed or non-conventionally packaged power systems, and state of the art solar power technology. These strategies will be required to meet the far more challenging thermal requirements of operating through a normal 28 day diurnal cycle. Limited battery survival temperature range remains the largest obstacle. C1 [Clark, P. E.; Millar, P. S.; Beaman, B.; Choi, M.; Cooper, L.; Feng, S.; King, R.; Leshin, L.; Lewis, R.; Yeh, P. S.; Young, E.; Lorenz, J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD USA. RP Clark, PE (reprint author), NASA, Goddard Space Flight Ctr, Code 695, Greenbelt, MD USA. EM 301-286-7457.pamela.e.clark@nasa.gov; john.e.lorenz@nasa.gov RI Millar, Pamela/B-4426-2013 NR 12 TC 0 Z9 0 U1 0 U2 3 PU AMER INST PHYSICS PI MELVILLE PA 2 HUNTINGTON QUADRANGLE, STE 1NO1, MELVILLE, NY 11747-4501 USA SN 0094-243X BN 978-0-7354-0639-1 J9 AIP CONF PROC PY 2009 VL 1103 BP 599 EP 607 PG 9 WC Engineering, Aerospace; Astronomy & Astrophysics; Energy & Fuels SC Engineering; Astronomy & Astrophysics; Energy & Fuels GA BJG15 UT WOS:000265592900071 ER PT S AU Clark, PE Curtis, SA Minetto, F Cheung, CY Keller, JF Moore, M Calle, CI AF Clark, P. E. Curtis, S. A. Minetto, F. Cheung, C. Y. Keller, J. F. Moore, M. Calle, C. I. BE Robertson, GA TI SPARCLE: Electrostatic Tool for Lunar Dust Control SO SPACE, PROPULSION & ENERGY SCIENCES INTERNATIONAL FORUM SPESIF-2009 SE AIP Conference Proceedings LA English DT Proceedings Paper CT 13th Conference on Thermophysics Applications in Microgravity/6th Symposium on New Frontiers in Space Propulsion Sciences/1st Symposium on Astrosociology CY FEB 24-26, 2009 CL Huntsville, AL SP Amer Astronaut Soc, Amer Inst Aeronaut & Astronaut, Astrosociol Res Inst DE Lunar Surface; Dust Control; Sampling; Electrostatic; Mechanical; Exploration ID SPACECRAFT; SURFACE; WAKE AB Successful exploration of most planetary surfaces, with their impact-generated dusty regoliths, will depend on the capabilities to keep surfaces free of the dust which could compromise performance and to collect dust for characterization. Solving the dust problem is essential before we return to the Moon. During the Apollo missions, the discovery was made that regolith fines, or dust, behaved like abrasive velcro, coating surfaces, clogging mechanisms, and making movement progressively more difficult as it was mechanically stirred up during surface operations, and abrading surfaces, including spacesuits, when attempts were made to remove it manually. In addition, some of the astronauts experienced breathing difficulties when exposed to dust that got into the crew compartment. The successful strategy will deal with dust dynamics resulting from interaction between mechanical and electrostatic forces. Here we will describe the surface properties of dust particles, the basis for their behavior, and an electrostatically-based approach and methodology for addressing this issue confirmed by our preliminary results. Our device concept utilizes a focused electron beam to control the electrostatic potential of the surface. A plate of the opposite potential is then used to induce dust migration in the presence of an electrical field. Our goal is a compact device of < 5 kg mass and using <5 watts of power to be operational in <5 years with heritage from ionic sweepers for active spacecraft potential control (e.g., on POLAR). Rovers could be fitted with devices that could harness the removal of dust for sampling as part of the extended exploration process on Mercury, Mars, asteroids or outer solar system satellites, as well as the Moon. C1 [Clark, P. E.] Catholic Univ Amer, Washington, DC 20064 USA. [Clark, P. E.; Curtis, S. A.; Minetto, F.; Keller, J. F.; Moore, M.] NASA, GSFC, Greenbelt, MD 20771 USA. [Calle, C. I.] NASA KSC, Code KT E, FL-32899 Cape Kennedy, Florida. RP Clark, PE (reprint author), Catholic Univ Amer, Washington, DC 20064 USA. EM pamela.clark@gsfc.nasa.gov RI Keller, John/I-5097-2013 FU NASA ESMD ETDP; NASA/KSC; NASA/GSDC IRAD; GSFC [695, 588] FX We would like to acknowledge the important discussion pertaining to this work we have had with our collegues William Farrell, David Carrier and Otto Berg. We thank NASA ESMD ETDP, NASA/KSC, NASA/GSDC IRAD, GSFC Codes 695, and 588 for their support. NR 30 TC 1 Z9 1 U1 0 U2 2 PU AMER INST PHYSICS PI MELVILLE PA 2 HUNTINGTON QUADRANGLE, STE 1NO1, MELVILLE, NY 11747-4501 USA SN 0094-243X BN 978-0-7354-0639-1 J9 AIP CONF PROC PY 2009 VL 1103 BP 608 EP 614 PG 7 WC Engineering, Aerospace; Astronomy & Astrophysics; Energy & Fuels SC Engineering; Astronomy & Astrophysics; Energy & Fuels GA BJG15 UT WOS:000265592900072 ER PT S AU Howard, RT Bryan, TC AF Howard, Richard T. Bryan, Thomas C. BE Robertson, GA TI The Next Generation Advanced Video Guidance Sensor: Flight Heritage and Current Development SO SPACE, PROPULSION & ENERGY SCIENCES INTERNATIONAL FORUM SPESIF-2009 SE AIP Conference Proceedings LA English DT Proceedings Paper CT 13th Conference on Thermophysics Applications in Microgravity/6th Symposium on New Frontiers in Space Propulsion Sciences/1st Symposium on Astrosociology CY FEB 24-26, 2009 CL Huntsville, AL SP Amer Astronaut Soc, Amer Inst Aeronaut & Astronaut, Astrosociol Res Inst DE Sensors; Docking; Automated; Proximity Operations; Relative Navigation; Rendezvous; Video AB The Next Generation Advanced Video Guidance Sensor (NGAVGS) is the latest in a line of sensors that have flown four times in the last 10 years. The NGAVGS has been under development for the last two years as a long-range proximity operations and docking sensor for use in an Automated Rendezvous and Docking (AR&D) system. The first autonomous rendezvous and docking in the history of the U.S. Space Program was successfully accomplished by Orbital Express, using the Advanced Video Guidance Sensor (AVGS) as the primary docking sensor. That flight proved that the United States now has a mature and flight proven sensor technology for supporting Crew Exploration Vehicles (CEV) and Commercial Orbital Transport Systems (COTS) Automated Rendezvous and Docking (AR&D). NASA video sensors have worked well in the past: the AVGS used on the Demonstration of Autonomous Rendezvous Technology (DART) mission operated successfully in "spot mode" out to 2 km, and the first generation rendezvous and docking sensor, the Video Guidance Sensor (VGS), was developed and successfully flown on Space Shuttle flights in 1997 and 1998. This paper presents the flight heritage and results of the sensor technology, some hardware trades for the current sensor, and discusses the needs of future vehicles that may rendezvous and dock with the International Space Station (ISS) and other Constellation vehicles. It also discusses approaches for upgrading AVGS to address parts obsolescence, and concepts for minimizing the sensor footprint, weight, and power requirements. In addition, the testing of the various NGAVGS development units will be discussed along with the use of the NGAVGS as a proximity operations and docking sensor. C1 [Howard, Richard T.; Bryan, Thomas C.] NASA, Automated Rendezvous & Docking Dev & Test Branch, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA. RP Howard, RT (reprint author), NASA, Automated Rendezvous & Docking Dev & Test Branch, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA. EM ricky.howard@nasa.gov NR 1 TC 0 Z9 0 U1 1 U2 1 PU AMER INST PHYSICS PI MELVILLE PA 2 HUNTINGTON QUADRANGLE, STE 1NO1, MELVILLE, NY 11747-4501 USA SN 0094-243X BN 978-0-7354-0639-1 J9 AIP CONF PROC PY 2009 VL 1103 BP 615 EP 621 PG 7 WC Engineering, Aerospace; Astronomy & Astrophysics; Energy & Fuels SC Engineering; Astronomy & Astrophysics; Energy & Fuels GA BJG15 UT WOS:000265592900073 ER PT S AU Broschart, SB Villac, BF AF Broschart, Stephen B. Villac, Benjamin F. BE Segerman, AM Lai, PC Wilkins, MP Pittelkau, ME TI IDENTIFICATION OF NON-CHAOTIC TERMINATOR ORBITS NEAR 6489 GOLEVKA SO SPACEFLIGHT MECHANICS 2009, VOL 134, PTS I-III SE Advances in the Astronautical Sciences LA English DT Proceedings Paper CT AAS/AIAA 19th Space Flight Mechanics Meeting CY FEB 08-12, 2009 CL Savannah, GA SP AAS, AIAA ID RADIATION PRESSURE; SATELLITE DYNAMICS; SOLAR-RADIATION; 2-BODY PROBLEM; STABILITY; ASTEROIDS; PARTICLES; MOTION AB Terminator orbits are an attractive class of quasi-periodic orbits for missions to small bodies because they exhibit stable behavior in the presence of a strong solar radiation pressure perturbation and robustness against uncertainty in the gravitational environment. Here, a numerical procedure is demonstrated for extracting long-term stability characteristics of terminator orbit dynamics. This approach yields a quantitative description of the region in state space that results in long-term stable terminator orbit dynamics in a high-fidelity dynamical model. These body-specific results complement the more generalized analytical results by providing more detail on the orbit stability properties in a particular situation of interest and stability information when the implicit assumptions of the analytical results do not apply. The procedure first identifies periodic orbits in the augmented Hill problem numerically, then evaluates the long-term behavior of nearby initial conditions using the Fast Lyapunov Indicator of chaoticity in a high-fidelity dynamical model that includes solar radiation pressure, an elliptical heliocentric small-body orbit, and a irregular rotating small-body gravity field. The procedure is successfully demonstrated on a model of the asteroid 6489 Golevka and results are compared with existing analytical results. This approach also has application to the study of orbiting particles and moons. C1 [Broschart, Stephen B.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Broschart, SB (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr,M-S 301-150, Pasadena, CA 91109 USA. EM Stephen.B.Broschart@ipl.nasa.gov; bvillac@uci.edu NR 28 TC 4 Z9 4 U1 0 U2 1 PU UNIVELT INC PI SAN DIEGO PA PO BOX 28130, SAN DIEGO, CA 92128 USA SN 1081-6003 BN 978-0-87703-554-1 J9 ADV ASTRONAUT SCI PY 2009 VL 134 BP 861 EP 880 PN I-III PG 20 WC Engineering, Aerospace SC Engineering GA BOE66 UT WOS:000276394400052 ER PT S AU Pelletier, FJ Antreasian, PG Ardalan, SM Criddle, KE Ionasescu, R Jacobson, RA Jones, JB Parcher, DW Roth, DC Thompson, PF AF Pelletier, Frederic J. Antreasian, Peter G. Ardalan, Shadan M. Criddle, Kevin E. Ionasescu, Rodica Jacobson, Robert A. Jones, Jeremy B. Parcher, Daniel W. Roth, Duane C. Thompson, Paul F. BE Segerman, AM Lai, PC Wilkins, MP Pittelkau, ME TI FLYING BY TITAN SO SPACEFLIGHT MECHANICS 2009, VOL 134, PTS I-III SE Advances in the Astronautical Sciences LA English DT Proceedings Paper CT AAS/AIAA 19th Space Flight Mechanics Meeting CY FEB 08-12, 2009 CL Savannah, GA SP AAS, AIAA AB The Cassini spacecraft encounters the massive Titan about once every month. These encounters are essential to the mission as Titan is the only satellite of Saturn that can provide enough gravity assist to shape the orbit tour, which will allow outstanding science for many years. From a navigation point of view, these encounters provide many challenges. In particular, those that fly close enough to the surface for the atmospheric drag to perturb the orbit. This paper discusses the dynamic models developed to successfully navigate Cassini and determine its trajectory. This includes the moon's gravity pull with its second degree zonal harmonics, J(2), the attitude control perturbations and the acceleration of drag. C1 [Pelletier, Frederic J.; Antreasian, Peter G.; Ardalan, Shadan M.; Criddle, Kevin E.; Ionasescu, Rodica; Jacobson, Robert A.; Jones, Jeremy B.; Parcher, Daniel W.; Roth, Duane C.; Thompson, Paul F.] CALTECH, Jet Prop Lab, Guidance Nav & Control Sect, Pasadena, CA 91109 USA. RP Pelletier, FJ (reprint author), CALTECH, Jet Prop Lab, Guidance Nav & Control Sect, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. NR 14 TC 0 Z9 0 U1 0 U2 0 PU UNIVELT INC PI SAN DIEGO PA PO BOX 28130, SAN DIEGO, CA 92128 USA SN 1081-6003 BN 978-0-87703-554-1 J9 ADV ASTRONAUT SCI PY 2009 VL 134 BP 1457 EP 1471 PN I-III PG 15 WC Engineering, Aerospace SC Engineering GA BOE66 UT WOS:000276394400088 ER PT S AU Williams, PN Ballard, CG Gist, EM Goodson, TD Hahn, Y Stumpf, PW Wagner, SV AF Williams, Powtawche N. Ballard, Christopher G. Gist, Emily M. Goodson, Troy D. Hahn, Yungsun Stumpf, Paul W. Wagner, Sean V. BE Segerman, AM Lai, PC Wilkins, MP Pittelkau, ME TI FLIGHT PATH CONTROL DESIGN FOR THE CASSINI EQUINOX MISSION SO SPACEFLIGHT MECHANICS 2009, VOL 134, PTS I-III SE Advances in the Astronautical Sciences LA English DT Proceedings Paper CT AAS/AIAA 19th Space Flight Mechanics Meeting CY FEB 08-12, 2009 CL Savannah, GA SP AAS, AIAA AB The Cassini-Huygens spacecraft has successfully completed its four-year Prime Mission and began a two-year extended mission on July 1, 2008. Officially named the "Equinox Mission", the extended mission includes 95 orbit trim maneuvers designed to achieve flybys of Titan, Enceladus, Rhea, and Dione. This paper gives an overview of maneuver statistical predictions and analysis for the Equinox Mission. C1 [Williams, Powtawche N.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Williams, PN (reprint author), CALTECH, Jet Prop Lab, Mail Stop 230-205,4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM Powtawche.N.Williams@jpl.nasa.gov NR 15 TC 0 Z9 0 U1 0 U2 1 PU UNIVELT INC PI SAN DIEGO PA PO BOX 28130, SAN DIEGO, CA 92128 USA SN 1081-6003 BN 978-0-87703-554-1 J9 ADV ASTRONAUT SCI PY 2009 VL 134 BP 1851 EP 1865 PN I-III PG 15 WC Engineering, Aerospace SC Engineering GA BOE66 UT WOS:000276394400111 ER PT B AU Wyatt, J Burleigh, S Jones, R Torgerson, L Wissler, S AF Wyatt, Jay Burleigh, Scott Jones, Ross Torgerson, Leigh Wissler, Steve GP IEEE TI Disruption Tolerant Networking Flight Validation Experiment on NASA's EPOXI Mission SO SPACOMN: 2009 FIRST INTERNATIONAL CONFERENCE ON ADVANCES IN SATELLITE AND SPACE COMMUNICATIONS LA English DT Proceedings Paper CT 1st International Conference on Advances in Satellite and Space Communications CY JUL 20-25, 2009 CL Colmar, FRANCE DE DTN; EPOXI; networking; protocols AB In October and November of 2008, the Jet Propulsion Laboratory installed and tested essential elements of Delay/Disruption Tolerant Networking (DTN) technology on the Deep Impact spacecraft. This experiment, called Deep Impact Network Experiment (DINET), was performed in close cooperation with the EPOXI project which has responsibility for the spacecraft. During DINET some 300 images were transmitted from the JPL nodes to the spacecraft. Then they were automatically forwarded from the spacecraft back to the JPL nodes, exercising DTN's bundle origination, transmission, acquisition, dynamic route computation, congestion control, prioritization, custody transfer, and automatic retransmission procedures, both on the spacecraft and on the ground, over a period of 27 days. All transmitted bundles were successfully received, without corruption. The DINET experiment demonstrated DTN readiness for operational use in space missions. This activity was part of a larger NASA space DTN development program to mature DTN to flight readiness for a wide variety of mission types by the end of 2011. This paper describes the DTN protocols, the flight demo implementation, validation metrics which were created for the experiment, and validation results. C1 [Wyatt, Jay; Burleigh, Scott; Jones, Ross; Torgerson, Leigh; Wissler, Steve] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Wyatt, J (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM E.Jay.Wyatt@jpl.nasa.gov; Scott.C.Burleigh@jpl.nasa.gov; Ross.M.Jones@jpl.nasa.gov; Jordan.L.Torgerson@jpl.nasa.gov; Steven.S.Wissler@jpl.nasa.gov NR 5 TC 11 Z9 11 U1 0 U2 2 PU IEEE PI NEW YORK PA 345 E 47TH ST, NEW YORK, NY 10017 USA BN 978-1-4244-4426-7 PY 2009 BP 187 EP 196 DI 10.1109/SPACOMM.2009.39 PG 10 WC Engineering, Electrical & Electronic; Telecommunications SC Engineering; Telecommunications GA BOZ33 UT WOS:000278100200033 ER PT S AU Cohn, SE AF Cohn, Stephen E. BE Temam, RM Tribbia, JJ TI Energetic Consistency and Coupling of the Mean and Covariance Dynamics SO SPECIAL VOLUME: COMPUTATIONAL METHODS FOR THE ATMOSPHERE AND THE OCEANS SE Handbook of Numerical Analysis LA English DT Article; Book Chapter ID ADJOINT VORTICITY EQUATION; VARIATIONAL ASSIMILATION; METEOROLOGICAL OBSERVATIONS; TRANSPORT SCHEMES; PREDICTION; CIRCULATION; MODEL C1 NASA, Goddard Space Flight Ctr, Global Modeling & Assimilat Off, Greenbelt, MD 20771 USA. RP Cohn, SE (reprint author), NASA, Goddard Space Flight Ctr, Global Modeling & Assimilat Off, Greenbelt, MD 20771 USA. NR 17 TC 2 Z9 2 U1 0 U2 0 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA SARA BURGERHARTSTRAAT 25, PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 1570-8659 BN 978-0-08-093103-6 J9 HANDB NUM ANAL PY 2009 VL 14 BP 443 EP 478 DI 10.1016/S1570-8659(08)00210-x PG 36 WC Mathematics SC Mathematics GA BCT26 UT WOS:000311344600012 ER PT J AU Enya, K Kotani, T Nakagawa, T Kataza, H Haze, K Higuchi, S Miyata, T Sako, S Nakamura, T Yamashita, T Narita, N Tamura, M Nishikawa, J Hayano, H Oya, S Itoh, Y Fukagawa, M Shibai, H Honda, M Baba, N Murakami, N Takami, M Matsuo, T Ida, S Abe, L Guyon, O Venet, M Yamamuro, T Bierden, P AF Enya, K. Kotani, T. Nakagawa, T. Kataza, H. Haze, K. Higuchi, S. Miyata, T. Sako, S. Nakamura, T. Yamashita, T. Narita, N. Tamura, M. Nishikawa, J. Hayano, H. Oya, S. Itoh, Y. Fukagawa, M. Shibai, H. Honda, M. Baba, N. Murakami, N. Takami, M. Matsuo, T. Ida, S. Abe, L. Guyon, O. Venet, M. Yamamuro, T. Bierden, P. CA SPICA Coronagraph Team BE Heras, AM swinyard, BM Isaak, KG Goicoechea, JR TI SPICA CORONAGRAPH INSTRUMENT (SCI) FOR THE DIRECT IMAGING AND SPECTROSCOPY OF EXO-PLANETS SO SPICA JOINT EUROPEAN/JAPANESE WORKSHOP LA English DT Proceedings Paper CT Joint European/Japanese Workshop on Space Infrared Telescope for Cosmology and Astrophysics CY JUL 06-08, 2009 CL Oxford, ENGLAND SP Daiwa Anglo-Japanese Fdn, Great Britain SASAKAWA Fdn DE SPICA; coronagraph; instrument; exo-planet; transit; spectroscopy ID STAR AB We present the SPICA Coronagraph Instrument (SCI) for the direct imaging and spectroscopy of exo-planets. The SPICA mission gives us a unique opportunity for high-contrast observations because of the large telescope aperture, the simple pupil shape, and the capability for infrared observations from space. The primary target of SCI is Jovian exo-planets. Using the spectroscopy mode of SCI, we will try the detection and the characterization of mid-infrared line features of the atmosphere of exo-planets. The specifications, performance and the design of the instrument are shown. The main wavelengths and the contrast required for the observations are 3.5-27 mu m, and 10(-6), respectively. We also show the progress of the development of key technology to realize SCI. Laboratory demonstration of the principle of coronagraph, realistic design and fabrication of masks, and the development of cryogenic active optics have been carried out, or are successfully ongoing. We are preparing a cryogenic chamber for the tests of the whole infrared coronagraph. A potentially important by-product of the instrument, transit monitoring for characterization of exo-planets, is also described. We expect that SCI will provide drastic progress in the understanding of various planetary systems and will be a unique capability in the SPICA era. C1 [Enya, K.; Kotani, T.; Nakagawa, T.; Kataza, H.; Haze, K.; Higuchi, S.] ISAS JAXA, 3-1-1 Yoshinodai, Kanagawa 2298510, Japan. [Haze, K.] Grad Univ Adv Studies, Dept Space & Astronaut Sci, Sagamihara, Kanagawa 2298510, Japan. [Higuchi, S.] Univ Tokyo, Grad Sch Sci, Dept Phys, Tokyo 1130033, Japan. [Miyata, T.; Sako, S.; Nakamura, T.] Univ Tokyo, Sch Sci, Inst Astron, Mitaka, Tokyo 1810015, Japan. [Yamashita, T.; Narita, N.; Tamura, M.; Nishikawa, J.; Hayano, H.; Oya, S.] Natl Astron Observ Japan, Mitaka, Tokyo 1818588, Japan. [Itoh, Y.] Kobe Univ, Grad Sch Sci, Kobe, Hyogo 6578501, Japan. [Fukagawa, M.; Shibai, H.] Osaka Univ, Grad Sch Sci, Dept Earth & Space Sci, Toyonaka, Osaka 5600043, Japan. [Honda, M.] Kanagawa Univ, Dept Informat Sci, Hiratsuka, Kanagawa 2591293, Japan. [Baba, N.; Murakami, N.] Hokkaido Univ, Div Appl Sci, Sapporo, Hokkaido 0608628, Japan. [Takami, M.] Acad Sinica, Inst Astron & Astrophys, Taipei, Taiwan. [Matsuo, T.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Ida, S.] Tokyo Inst Technol, Dept Earth & Space Sci, Tokyo 1528551, Japan. [Abe, L.] Univ Nice, CNRS, Lab AH Fizeau, F-06108 Nice, France. [Guyon, O.] Natl Inst Nat Sci, Natl Astron Observ Japan, Subaru Telescope, Hilo, HI 96720 USA. [Venet, M.] Observ Astron Marseille Provence, F-13388 Marseille, France. [Yamamuro, T.; Bierden, P.] Optcraft Corp, Sagamihara, Kanagawa 2291104, Japan. [SPICA Coronagraph Team] Boston Micromachines Corp, Cambridge, MA 02138 USA. RP Enya, K (reprint author), ISAS JAXA, 3-1-1 Yoshinodai, Kanagawa 2298510, Japan. NR 11 TC 0 Z9 0 U1 1 U2 1 PU E D P SCIENCES PI CEDEX A PA 17 AVE DU HOGGAR PARC D ACTIVITES COUTABOEUF BP 112, F-91944 CEDEX A, FRANCE BN 978-2-7598-0493-1 PY 2009 AR UNSP 01004 DI 10.1051/spica/200901004 PG 6 WC Astronomy & Astrophysics; Instruments & Instrumentation SC Astronomy & Astrophysics; Instruments & Instrumentation GA BUU69 UT WOS:000290389800004 ER PT S AU Nixon, DD Johnson, CD AF Nixon, D. D. Johnson, C. D. GP IEEE TI Numerical Evaluation of the "Dual-Kernel, Counter-flow" Matric Convolution Integral that Arises in Discrete/Continuous (D/C) Control Theory SO SSST: 2009 41ST SOUTHEASTERN SYMPOSIUM ON SYSTEM THEORY SE Southeastern Symposium on System Theory LA English DT Proceedings Paper CT 41st Southeastern Symposium on System Theory CY MAR 15-17, 2009 CL Tullahoma, TN AB Discrete/Continuous (D/C) control theory is a new generalized theory of discrete-time control that expands the concept of conventional (exact) discrete-time control so that actuator commands need not be constant between control decisions, but can be more generally defined and implemented as functions that vary with time across each sample period in some beneficial manner. Because the plant/control system construct contains two linear subsystems arranged in tandem, a novel "dual-kernel counter-flow" convolution integral appears in the formulation; and, as part of the D/C control design and implementation process, numerical evaluation of that integral over each sample period is required. Three fundamentally different evaluation methods and associated algorithms are derived for the constant-coefficient case, and numerical results are matched against three available examples that have closed-form solutions. C1 [Nixon, D. D.] NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA. [Johnson, C. D.] Univ Alabama, Elect & Comp Engn, Huntsville, AL 35899 USA. RP Nixon, DD (reprint author), NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA. EM douglas.d.nixon@nasa.gov; johnson@ece.uah.edu NR 9 TC 1 Z9 1 U1 0 U2 0 PU IEEE PI NEW YORK PA 345 E 47TH ST, NEW YORK, NY 10017 USA SN 0094-2898 BN 978-1-4244-3324-7 J9 SE SYM SYS THRY PY 2009 BP 285 EP + PG 2 WC Computer Science, Artificial Intelligence; Computer Science, Hardware & Architecture; Computer Science, Theory & Methods; Robotics SC Computer Science; Robotics GA BKN37 UT WOS:000268672400057 ER PT S AU Hannan, MR Johnson, CD AF Hannan, Michael R. Johnson, C. D. GP IEEE TI Simulation and Animation of Coffee Sloshing in a Cup; A Testbed for Control Design SO SSST: 2009 41ST SOUTHEASTERN SYMPOSIUM ON SYSTEM THEORY SE Southeastern Symposium on System Theory LA English DT Proceedings Paper CT 41st Southeastern Symposium on System Theory CY MAR 15-17, 2009 CL Tullahoma, TN DE Dual-Mode Control; Disturbance-Observer; Disturbance-Accommodation; Animation; GUI; LQR; Controls Education; Simulink AB This paper describes a software tool useful for gaining insight into the trade-offs encountered in any control system design and to the benefits of a dual-mode control when needed The plant is a relatively simple two body problem (two masses coupled with a spring & damper). A GUI interfaces with a Simulink (R) model of the plant and two control options. The GUI makes it possible to switch controllers as the simulation is running and illustrates the trade-offs between performance (output tracking) and control energy management. The dynamics are presented in the form of coffee sloshing in a cup to give the user a familiar physical interpretation. C1 [Hannan, Michael R.] NASA MSFC, Huntsville, AL 35811 USA. [Johnson, C. D.] Univ Alabama, ECE Dept, Huntsville, AL USA. RP Hannan, MR (reprint author), NASA MSFC, Huntsville, AL 35811 USA. NR 5 TC 0 Z9 0 U1 0 U2 0 PU IEEE PI NEW YORK PA 345 E 47TH ST, NEW YORK, NY 10017 USA SN 0094-2898 BN 978-1-4244-3324-7 J9 SE SYM SYS THRY PY 2009 BP 317 EP + DI 10.1109/SSST.2009.4806826 PG 2 WC Computer Science, Artificial Intelligence; Computer Science, Hardware & Architecture; Computer Science, Theory & Methods; Robotics SC Computer Science; Robotics GA BKN37 UT WOS:000268672400063 ER PT S AU Creech-Eakman, MJ Hora, J Ivezic, Z Jurgenson, C Luttermoser, D Marengo, M Speck, A Stencel, R Thompson, RR AF Creech-Eakman, M. J. Hora, J. Ivezic, Z. Jurgenson, C. Luttermoser, D. Marengo, M. Speck, A. Stencel, R. Thompson, R. R. BE Guzik, JA Bradley, PA TI Multiwavelength Study of Pulsation and Dust Production in Mira Variables Using Optical Interferometry for Constraints SO STELLAR PULSATION: CHALLENGES FOR THEORY AND OBSERVATION SE AIP Conference Proceedings LA English DT Proceedings Paper CT International Conference on Stellar Pulsation - Challenges for Theory and Observation CY MAY 31-JUN 05, 2009 CL Santa Fe, NM SP Los Alamos Natl Lab, Ctr Space Sci & Explorat, Inst Geophys & Planetary Phys, TAE Photo & Design, La Fonda Plaza DE mira variables; dust production; infrared spectroscopy; optical/infrared interferometry; facility: Spitzer Space Telescope facility: Palomar Testbed Interferometer ID TIME-VARIATION; STARS AB Optical interferometry is a technique by which the diameters and indeed the direct pulsations of stars are routinely being measured. As a follow-on to a 7 year interferometric campaign to measure the pulsations of over 100 mira variables, our team has been using the Spitzer Space Telescope to obtain 95 mid-infrared spectra of 25 miras during their pulsations over one year while simultaneously ascertaining their near-infrared diameters using the Palomar Testbed Interferometer. These data will then be combined with modeling from NLTE and radiative transfer codes to place hard constraints on our understanding of these stars and their circumstellar environments. We present some initial results from this work and discuss the next steps toward fully characterizing the atmosphere, molecular photosphere and dust production in mira variables. C1 [Creech-Eakman, M. J.] New Mexico Inst Min & Technol, Dept Phys, 801 Leroy Pl, Socorro, NM 87801 USA. [Creech-Eakman, M. J.; Jurgenson, C.] Magdalena Ridge Observ Interferometer, Socorro, NM 87801 USA. [Hora, J.; Marengo, M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Ivezic, Z.] Univ Washington, Dept Astron, Seattle, WA 98195 USA. [Luttermoser, D.] East Tennessee State Univ, Dept Phys, Johnson City, TN 37614 USA. [Marengo, M.] Iowa State Univ, Dept Phys, Ames, IA 50011 USA. [Speck, A.] Univ Missouri, Dept Phys & Astron, Columbia, MO 65211 USA. [Stencel, R.] Univ Denver, Dept Phys & Astrophys, Denver, CO 80208 USA. [Thompson, R. R.] NASA, Opt Sci Corp, SOFIA Project, Dryden Aircraft Operat Fac, Palmdal, CA 93550 USA. RP Creech-Eakman, MJ (reprint author), New Mexico Inst Min & Technol, Dept Phys, 801 Leroy Pl, Socorro, NM 87801 USA. OI Hora, Joseph/0000-0002-5599-4650 FU NASA grant to the PI and team associated with Spitzer program [GO50717] FX Some of the work on this project was supported through a NASA grant to the PI and team associated with Spitzer program GO50717. NR 14 TC 0 Z9 0 U1 0 U2 0 PU AMER INST PHYSICS PI MELVILLE PA 2 HUNTINGTON QUADRANGLE, STE 1NO1, MELVILLE, NY 11747-4501 USA SN 0094-243X BN 978-0-7354-0707-7 J9 AIP CONF PROC PY 2009 VL 1170 BP 137 EP + PG 2 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BPW04 UT WOS:000280126200030 ER PT J AU Kaul, UK AF Kaul, Upender K. TI Modeling and Simulation of Normal and Damage Vibration Signatures of Idealized Gears SO STRUCTURAL HEALTH MONITORING-AN INTERNATIONAL JOURNAL LA English DT Article DE wave-based structural health monitoring; damage vibration signatures; finite-difference modeling; elastodynamic partial differential equations ID WAVE PROPAGATION; MEDIA AB A physics-based first principles approach is adopted in this study to simulate vibration signatures from an idealized gear such as a thin spur gear under plane dynamic stresses induced by an impulsive rotation. The governing equations of velocity-stress are solved using a finite-difference formulation in generalized curvilinear coordinates and a fully characteristic set of boundary conditions based on the theory of hyperbolic systems. The vibration signatures are thus directly obtained in the time domain. A second-order accurate in time and space, time-staggered leapfrog scheme, is used to integrate the time-dependent partial differential equations. Normal as well as damage signatures are obtained and compared; normal signatures correspond to uniform material properties of the gear, and damage signatures correspond to one of the gear teeth being made less rigid in a certain fashion so as to mimic a damage such as due to impact-induced pitting, deformation or incipient crack formation. It is observed that significant deviations from the normal signature occur in amplitude due to this seeded damage. Using this approach, baseline or reference vibration signatures can be obtained for any structural subsystem to aid in its health monitoring. C1 NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Kaul, UK (reprint author), NASA, Ames Res Ctr, MS 258-5, Moffett Field, CA 94035 USA. EM Upender.K.Kaul@nasa.gov FU NASA Computing, Information and Communications Technology (CICT) Program FX This work was supported by the NASA Computing, Information and Communications Technology (CICT) Program. NR 17 TC 2 Z9 2 U1 0 U2 1 PU SAGE PUBLICATIONS LTD PI LONDON PA 1 OLIVERS YARD, 55 CITY ROAD, LONDON EC1Y 1SP, ENGLAND SN 1475-9217 J9 STRUCT HEALTH MONIT JI Struct. Health Monit. PD JAN PY 2009 VL 8 IS 1 BP 17 EP 28 DI 10.1177/1475921708094791 PG 12 WC Engineering, Multidisciplinary; Instruments & Instrumentation SC Engineering; Instruments & Instrumentation GA 398XB UT WOS:000262763700002 ER PT J AU Crespo, LG Giesy, DP Kenny, SP AF Crespo, Luis G. Giesy, Daniel P. Kenny, Sean P. TI Reliability-based analysis and design via failure domain bounding SO STRUCTURAL SAFETY LA English DT Article DE Reliability; Bounds; Failure probability; Optimization ID ALGORITHM; SYSTEMS AB This paper proposes a methodology for bounding and approximating failure probabilities for systems with parametric uncertainty that are subject to multiple design requirements. The two fundamental developments in this work are (1) a method to explicitly compute upper bounds on failure probability based on solving an optimization problem, and (2) a hybrid method, utilizing the upper bounds together with conditional sampling, to achieve highly accurate estimates of failure probabilities. The computation of failure probability bounds is accomplished by the deformation of hyper-spherical or hyper-rectangular sets in the standard normal space and utilizes a combination of numerical optimization and analytic tools. The methods for calculating these bounds are applicable to systems having multiple limit state functions and are not subject to difficulties when there are multiple critical parameter points. Numerical experiments are presented to demonstrate that the gains in accuracy and efficiency of the method are considerable when compared to alternative methods. The tools proposed are especially suited for design optimization due to their efficiency and the resulting continuity of the upper bounds. Since only standard optimization algorithms are required for implementation, these strategies are easily applicable to a variety of complex engineering problems. Published by Elsevier Ltd. C1 [Crespo, Luis G.] Natl Inst Aerospace, Hampton, VA 23666 USA. [Giesy, Daniel P.; Kenny, Sean P.] NASA, Langley Res Ctr, Hampton, VA 23681 USA. RP Crespo, LG (reprint author), Natl Inst Aerospace, 100 Explorat Way, Hampton, VA 23666 USA. EM lgcrespo@nianet.org; daniel.p.giesy@nasa.gov; sean.p.kenny@nasa.gov NR 24 TC 7 Z9 7 U1 0 U2 1 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0167-4730 J9 STRUCT SAF JI Struct. Saf. PY 2009 VL 31 IS 4 BP 306 EP 315 DI 10.1016/j.strusafe.2008.09.001 PG 10 WC Engineering, Civil SC Engineering GA 448IG UT WOS:000266255700005 ER PT B AU Lis, DC Goldsmith, PF Bergin, EA Falgarone, E Gerin, M Roueff, E AF Lis, Dariusz C. Goldsmith, Paul F. Bergin, Edwin A. Falgarone, Edith Gerin, Maryvonne Roueff, Evelyne BE Lis, DC Vaillancourt, JE Goldsmith, PF Bell, TA Scoville, NZ Zmuidzinas, J TI Hydrides in Space: Past, Present, and Future SO SUBMILLIMETER ASTROPHYSICS AND TECHNOLOGY: A SYMPOSIUM HONORING THOMAS G. PHILLIPS SE Astronomical Society of the Pacific Conference Series LA English DT Proceedings Paper CT Symposium on Submillimeter Astrophysics and Technology held in honor of Thomas G Philllips CY FEB 23-24, 2009 CL Calif Inst Technol, Pasadena, CA HO Calif Inst Technol ID O1 HALE-BOPP; DENSE INTERSTELLAR CLOUDS; 1996 B2 HYAKUTAKE; PRESTELLAR CORES; DEUTERIUM FRACTIONATION; PHYSICAL CONDITIONS; DEUTERATED AMMONIA; HYDROGEN-CHLORIDE; STARLESS CORES; CO DEPLETION AB One of the central questions of modern astrophysics concerns the life cycle of molecules in the Universe-from the diffuse interstellar medium to planetary systems-and the chemical pathways leading from simple atoms and diatomic molecules to complex organic species. In the past two decades, the Caltech Submillimeter Observatory (CSO) has contributed a number of key discoveries on these topics. Light hydrides are of particular interest for astrochemistry, as the basic building blocks of the chemical networks in both diffuse and dense clouds. Ongoing and planned submillimeter wide-field continuum surveys will yield hundreds of potential galactic targets suitable for detailed spectroscopic follow-ups. Recent advances in detector and digital spectrometer technologies promise to truly revolutionize further the field of high-resolution submillimeter spectroscopy and its application to the study of the life cycle of molecules. This will greatly improve our understanding of astrochemistry, astrobiology, the origin of life on Earth, and allow assessing the possibilities of life in other planetary systems. C1 [Lis, Dariusz C.] CALTECH, MS 301-17, Pasadena, CA 91125 USA. [Goldsmith, Paul F.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Bergin, Edwin A.] Univ Michigan, Ann Arbor, MI 48109 USA. [Falgarone, Edith; Gerin, Maryvonne] CNRS, LERMA, F-75231 Paris, France. [Falgarone, Edith; Gerin, Maryvonne] Ecole Normale Super, F-75231 Paris, France. [Roueff, Evelyne] Observ Paris, F-92195 Meudon, France. RP Lis, DC (reprint author), CALTECH, MS 301-17, Pasadena, CA 91125 USA. EM dcl@caltech.edu; paul.f.goldsmith@jpl.nasa.gov; ebergin@umich.edu; edith@lra.ens.fr; gerin@lra.ens.fr FU NSF [AST-0540882] FX The Caltech submillimted Observatory is supported by NSF grant AST-0540882. NR 52 TC 9 Z9 9 U1 0 U2 4 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 978-1-58381-714-8 J9 ASTR SOC P PY 2009 VL 417 BP 23 EP + PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BQL34 UT WOS:000281244000003 ER PT B AU Langer, WD AF Langer, William D. BE Lis, DC Vaillancourt, JE Goldsmith, PF Bell, TA Scoville, NZ Zmuidzinas, J TI The Lifecycle of Carbon in the Interstellar Medium SO SUBMILLIMETER ASTROPHYSICS AND TECHNOLOGY: A SYMPOSIUM HONORING THOMAS G. PHILLIPS SE Astronomical Society of the Pacific Conference Series LA English DT Proceedings Paper CT Symposium on Submillimeter Astrophysics and Technology held in honor of Thomas G Philllips CY FEB 23-24, 2009 CL Calif Inst Technol, Pasadena, CA HO Calif Inst Technol ID GALACTIC PLANE SURVEY; MOLECULAR CLOUDS; ATOMIC CARBON; CO SURVEY; CHEMISTRY; LINE AB This review summarizes the role of gaseous carbon in the Galactic interstellar medium (ISM) as a tracer of its different phases and as a primary gas coolant. Carbon in one of its many gaseous atomic and molecular forms has proven to be critical to our ability to trace the chemical and physical states of the cloud. This review covers the important role that Professor Tom Phillips has played in the study of key carbon species in the ISM. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Langer, WD (reprint author), CALTECH, Jet Prop Lab, MS 180-500,4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM william.langer@jpl.nasa.gov NR 22 TC 0 Z9 0 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 978-1-58381-714-8 J9 ASTR SOC P PY 2009 VL 417 BP 71 EP 82 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BQL34 UT WOS:000281244000006 ER PT B AU Becklin, EE Gehrz, RD AF Becklin, E. E. Gehrz, R. D. BE Lis, DC Vaillancourt, JE Goldsmith, PF Bell, TA Scoville, NZ Zmuidzinas, J TI SOFIA: Stratospheric Observatory for Infrared Astronomy SO SUBMILLIMETER ASTROPHYSICS AND TECHNOLOGY: A SYMPOSIUM HONORING THOMAS G. PHILLIPS SE Astronomical Society of the Pacific Conference Series LA English DT Proceedings Paper CT Symposium on Submillimeter Astrophysics and Technology held in honor of Thomas G Philllips CY FEB 23-24, 2009 CL Calif Inst Technol, Pasadena, CA HO Calif Inst Technol ID SPACE-TELESCOPE; MISSION AB The NASA/DLR. Stratospheric Observatory for Infrared Astronomy (SOFIA) is a 2.5 m infrared telescope in a Boeing 747SP. Flying at altitudes as high as 45,000 feet, it will enable 0.3 mu m - 1.6 mm observations with an average transmission of >= 80%. We describe the key role that Toni Phillips played in the early days of airborne astronomy that culminated in the development of SOFIA. The facility design and status are described. Nine first generation instruments that will fly on SOFIA include broadband imaging cameras, moderate resolution spectrographs capable of resolving emission features due to dust and large molecules, and high resolution spectrometers suitable for kinematical studies of molecular and atomic gas lines at km s(-1) resolution. World-wide deployments will provide access to the entire sky and enable timely observations of transient events. SOFIA's sensitivity for imaging and spectroscopy is similar to that of the space observatory ISO. Its telescope is diffraction-limited beyond 25 mu m, making its iinages 3 times sharper than those obtained by the Spitzer Space Telescope at these wavelengths. We describe the characteristics of the observatory and give several examples of science opportunities with SOFIA. C1 [Becklin, E. E.] NASA, Univ Space Res Assoc, Ames Res Ctr, MS 211-3, Moffett Field, CA 94035 USA. RP Becklin, EE (reprint author), NASA, Univ Space Res Assoc, Ames Res Ctr, MS 211-3, Moffett Field, CA 94035 USA. EM becklin@astro.ucla.edu NR 10 TC 4 Z9 4 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 978-1-58381-714-8 J9 ASTR SOC P PY 2009 VL 417 BP 101 EP + PG 2 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BQL34 UT WOS:000281244000009 ER PT B AU Benford, DJ AF Benford, Dominic J. BE Lis, DC Vaillancourt, JE Goldsmith, PF Bell, TA Scoville, NZ Zmuidzinas, J TI The SOFIA/SAFIRE Far-Infrared Spectrometer: Highlighting Submillimeter Astrophysics and Technology SO SUBMILLIMETER ASTROPHYSICS AND TECHNOLOGY: A SYMPOSIUM HONORING THOMAS G. PHILLIPS SE Astronomical Society of the Pacific Conference Series LA English DT Proceedings Paper CT Symposium on Submillimeter Astrophysics and Technology held in honor of Thomas G Philllips CY FEB 23-24, 2009 CL Calif Inst Technol, Pasadena, CA HO Calif Inst Technol AB The Submillimeter and Far-InfraRed Experiment (SAFIRE) on the SOFIA airborne observatory is an imaging spectrometer for wavelengths between 28 mu m and 440 mu m. Our design is a dual-band long-slit grating spectrometer, which provides broadband (similar to 4000 km/s) observations in two lines simultaneously over a field of view roughly 10 '' wide by 320 '' long. The low backgrounds in spectroscopy require very sensitive detectors with noise equivalent powers of order 10(-18) W/root Hz. We are developing a kilopixel, filled detector array for SAFIRE in a 32 x 40 format. The detector consists of a transition edge sensor (TES) bolometer array, a per-pixel broadband absorbing backshort array, and a NIST SQUID multiplexer readout array. This general type of array has been used successfully in the GISMO instrument, so we extrapolate to the sensitivity needed for airborne spectroscopy. Much of the cryogenic, electronics, and software infrastructure for SAFIRE have been developed. I provide here an overview of the progress on SAFIRE. C1 NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Benford, DJ (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. EM dominic.benford@nasa.gov RI Benford, Dominic/D-4760-2012 OI Benford, Dominic/0000-0002-9884-4206 NR 6 TC 0 Z9 0 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 978-1-58381-714-8 J9 ASTR SOC P PY 2009 VL 417 BP 137 EP 142 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BQL34 UT WOS:000281244000013 ER PT B AU Goldsmith, PF Velusamy, T Li, D Langer, W AF Goldsmith, Paul F. Velusamy, T. Li, Di Langer, William BE Lis, DC Vaillancourt, JE Goldsmith, PF Bell, TA Scoville, NZ Zmuidzinas, J TI H-2 in Molecular Clouds SO SUBMILLIMETER ASTROPHYSICS AND TECHNOLOGY: A SYMPOSIUM HONORING THOMAS G. PHILLIPS SE Astronomical Society of the Pacific Conference Series LA English DT Proceedings Paper CT Symposium on Submillimeter Astrophysics and Technology held in honor of Thomas G Philllips CY FEB 23-24, 2009 CL Calif Inst Technol, Pasadena, CA HO Calif Inst Technol ID HYDROGEN; GAS AB We report the detection of the S(0) and S(1) pure rotational transitions of H-2 in emission from a boundary layer of the Taurus molecular cloud. These lines were observed with the Spitzer Infrared Spectrograph (IRS), and are very weak, with maximum specific intensity <= 0.4 MJy sr(-1). The emission is strongest 8.5' (0.33 pc) outside the edge of the cloud defined by the (CO)-C-13. We see H2 emission towards the bulk of the cloud at a lower level, suggestive of limb brightening of an envelope around the purely molecular cloud. The peak column densities looking directly towards the cloud are N(J = 3) = 1.3x10(17) cm(-2), and N(J = 2) = 2.2x10(18) cm(-2). Towards the maximum of the rotationally excited H-2 emission, N(J = 3) = 5.2x10(17) cm(-2) and N(J = 2) = 4.4x10(18) cm(-2). Interpreting the ratio is made difficult by the not well determined ortho- to para-H-2 ratio (OPR), but for reasonable values of the OPR, we can constrain the characteristics of the region responsible for the H2 emission. For example, for OPR = 3 and n(H-2) = 100 cm(-3), T-K must be greater than approximately 200 K. We have used the Meudon PDR code to model the H-2 emission from the cloud edge, and find that while the column density in J = 2 can be reproduced with reasonable parameters for the region and its environment, the column density in J = 3 that is predicted falls more than a factor of 5 below that observed. This suggests that an additional source of H-2 excitation is present. Further data and modeling are required to understand this issue, which will improve our understanding of cloud structure and the physics of H-2 formation. C1 [Goldsmith, Paul F.] CALTECH, Jet Prop Lab, Oak Grove Dr,MS 180-703, Pasadena, CA 91103 USA. RP Goldsmith, PF (reprint author), CALTECH, Jet Prop Lab, Oak Grove Dr,MS 180-703, Pasadena, CA 91103 USA. EM paul.f.goldsmith@jpl.nasa.gov; velusamy@jpl.nasa.gov; dili@jpl.nasa.gov; william.langer@jpl.nasa.gov NR 13 TC 0 Z9 0 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 978-1-58381-714-8 J9 ASTR SOC P PY 2009 VL 417 BP 177 EP + PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BQL34 UT WOS:000281244000017 ER PT B AU Pearson, JC Brauer, CS Drouin, BJ Yu, S AF Pearson, J. C. Brauer, C. S. Drouin, B. J. Yu, S. BE Lis, DC Vaillancourt, JE Goldsmith, PF Bell, TA Scoville, NZ Zmuidzinas, J TI Better Spectrometers, Beautiful Spectra, and Confusion for All SO SUBMILLIMETER ASTROPHYSICS AND TECHNOLOGY: A SYMPOSIUM HONORING THOMAS G. PHILLIPS SE Astronomical Society of the Pacific Conference Series LA English DT Proceedings Paper CT Symposium on Submillimeter Astrophysics and Technology held in honor of Thomas G Philllips CY FEB 23-24, 2009 CL Calif Inst Technol, Pasadena, CA HO Calif Inst Technol ID ORION AB The confluence of enormous improvements in submillimeter receivers and the development of powerful large scale observatories is about to force astrophysics and the sciences that support it to develop novel approaches for interpretation of data. The historical method of observing one or two lines and carefully analyzing them in the context of a simple model is now only applicable for distant objects where only a few lines are strong enough to be observable. Modern observatories collect many GHz of high signal-to-noise spectra in a single observation and, in many cases, at sufficiently high spatial resolution to start resolving chemically distinct regions. The observatories planned for the near future and the inevitable upgrades of existing facilities will make large spectral data sets the rule rather than the exception in many areas of molecular astrophysics. The methodology and organization required to fully extract the available information and interpret these beautiful spectra represents a challenge to submillimeter astrophysics similar in magnitude to the last few decades of effort in improving receivers. The quality and abundance of spectra effectively prevents line-by-line analysis from being a time efficient proposition, however, global analysis of complex spectra is a science in its infancy. Spectroscopy at several other wavelengths has developed a number of techniques to analyze complex spectra, which can provide a great deal of guidance to the molecular astrophysics community on how to attack the complex spectrum problem. Ultimately, the challenge is one of organization, similar to building observatories, requiring teams of specialists combining their knowledge of dynamical, structural, chemical and radiative models with detailed knowledge in molecular physics and gas and grain surface chemistry to extract and exploit the enormous information content of complex spectra. This paper presents a spectroscopist's view of the necessary elements in a tool for complex spectral analysis. C1 [Pearson, J. C.; Brauer, C. S.; Drouin, B. J.; Yu, S.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Pearson, JC (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM john.c.pearson@jpl.nasa.gov NR 8 TC 0 Z9 0 U1 0 U2 1 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 978-1-58381-714-8 J9 ASTR SOC P PY 2009 VL 417 BP 191 EP 202 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BQL34 UT WOS:000281244000018 ER PT B AU Bradford, CM Aguirre, JE Bock, JJ Earle, L Glenn, J Inami, H Kamenetzky, J Maloney, PR Matsuhara, H Naylor, BJ Nguyen, HT Zmuidzinas, J AF Bradford, C. M. Aguirre, J. E. Bock, J. J. Earle, L. Glenn, J. Inami, H. Kamenetzky, J. Maloney, P. R. Matsuhara, H. Naylor, B. J. Nguyen, H. T. Zmuidzinas, J. BE Lis, DC Vaillancourt, JE Goldsmith, PF Bell, TA Scoville, NZ Zmuidzinas, J TI Survey Spectroscopy in the Submillimeter and Millimeter, from the CSO to CCAT SO SUBMILLIMETER ASTROPHYSICS AND TECHNOLOGY: A SYMPOSIUM HONORING THOMAS G. PHILLIPS SE Astronomical Society of the Pacific Conference Series LA English DT Proceedings Paper CT Symposium on Submillimeter Astrophysics and Technology held in honor of Thomas G Philllips CY FEB 23-24, 2009 CL Calif Inst Technol, Pasadena, CA HO Calif Inst Technol ID INITIAL MASS FUNCTION; CLOVERLEAF QUASAR; STAR-FORMATION; MOLECULAR GAS; BROAD-BAND; Z-SPEC; SPECTROMETER; EMISSION; REDSHIFT; GALAXIES AB I outline some results from the Z-Spec instrument at the CSO and present a concept for CCAT survey spectrometer. C1 [Bradford, C. M.; Bock, J. J.; Naylor, B. J.; Nguyen, H. T.; Zmuidzinas, J.] CALTECH, Jet Prop Lab, JPL Mail Code 169-506,4800 Oak Grove Dr, Pasadena, CA 91109 USA. [Bradford, C. M.; Bock, J. J.; Naylor, B. J.; Zmuidzinas, J.] CALTECH, Pasadena, CA 91125 USA. [Aguirre, J. E.; Earle, L.; Glenn, J.; Kamenetzky, J.; Maloney, P. R.] Univ Colorado, Boulder, CO 80303 USA. [Aguirre, J. E.] Univ Penn, Philadelphia, PA 19104 USA. [Inami, H.; Matsuhara, H.] Japan Aerosp & Explorat Agcy, Inst Space & Astronaut Sci, Sagamihara, Kanagawa, Japan. RP Bradford, CM (reprint author), CALTECH, Jet Prop Lab, JPL Mail Code 169-506,4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM bradford@submm.caltech.edu; jason.glenn@colorado.edu; jonas@submm.caltech.edu NR 21 TC 3 Z9 3 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 978-1-58381-714-8 J9 ASTR SOC P PY 2009 VL 417 BP 341 EP + PG 3 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BQL34 UT WOS:000281244000034 ER PT B AU Staguhn, J Benford, D Allen, C Arendt, R George, J Fixsen, D Maher, S Sharp, E Ames, T Chuss, D Dwek, E Marx, C Miller, T Moseley, SH Navarro, S Schinnerer, E Sievers, A Walter, F Wollack, E AF Staguhn, Johannes Benford, Dominic Allen, Christine Arendt, Rick George, Jithin Fixsen, Dale Maher, Stephen Sharp, Elmer Ames, Troy Chuss, David Dwek, Eli Marx, Catherine Miller, Tim Moseley, S. Harvey Navarro, Santiago Schinnerer, Eva Sievers, Albrecht Walter, Fabian Wollack, Edward BE Lis, DC Vaillancourt, JE Goldsmith, PF Bell, TA Scoville, NZ Zmuidzinas, J TI New Results from GISMO, a 2 mm Camera Using a Backshort-Under-Grid TES Bolometer Array SO SUBMILLIMETER ASTROPHYSICS AND TECHNOLOGY: A SYMPOSIUM HONORING THOMAS G. PHILLIPS SE Astronomical Society of the Pacific Conference Series LA English DT Proceedings Paper CT Symposium on Submillimeter Astrophysics and Technology held in honor of Thomas G Philllips CY FEB 23-24, 2009 CL Calif Inst Technol, Pasadena, CA HO Calif Inst Technol AB In October 2008, we demonstrated for the second time our 2 mm bolometer camera GISMO (the Goddard IRAM Superconducting 2 Millimeter Observer) for astronomical observations at the IRAM 30 m telescope in Spain. GISMO uses a monolithic 8 x 16 Backshort Under Grid (BUG) array with superconducting Transition Edge Sensors (TES). The instrument's fast beam yields 0.9 lambda/D pixel sampling, which optimizes GISMO for detecting sources serendipitously in large sky surveys, while the capability for diffraction limited imaging is preserved. In order to ensure GISMO's operation under all weather conditions, we used a 40% neutral density filter at 4 K. In less than ideal weather conditions we obtained map sensitivities for the working pixels of between 40 mJy s(-1/2) and 50 mJy s(-1/2). These numbers are consistent with our atmospheric model calculations. The predicted map NEFDs range from 28 to 56 mJy s(-1/2) for GISMO's optical configuration (including the 40% neutral density filter) and observing conditions ranging between 10% and 40% line of sight opacities. With an optimized observing strategy for point sources of known position, this sensitivity can further be increased by a factor of 1.5, which we demonstrate by means of analyzing of our signal to noise ratio achieved for point source crossings in the time stream data. The noise in our co-added maps (with few thousand seconds of integration time) scales very well with the square root of time clown to sub-mJy levels. We have now designed a cryogenic mechanism that will allow us to move neutral density filters in or out of the beam during future observations. Our simulations indicate that we will gain a factor of 2.4 in observing efficiency if we take out the neutral density filter under good weather conditions. Under typical conditions (20% line of sight sky opacity) we expect to achieve a good pixel map sensitivity of 22 mJy s(-1/2) and a map NEFD of 1 mJy in an observation lasting about 8 minutes. C1 [Staguhn, Johannes; Benford, Dominic; Allen, Christine; Arendt, Rick; Fixsen, Dale; Maher, Stephen; Sharp, Elmer; Ames, Troy; Chuss, David; Dwek, Eli; Marx, Catherine; Miller, Tim; Moseley, S. Harvey; Wollack, Edward] NASA, Goddard Space Flight Ctr, Observat Cosmol Lab, Code 665, Greenbelt, MD 20771 USA. RP Staguhn, J (reprint author), NASA, Goddard Space Flight Ctr, Observat Cosmol Lab, Code 665, Greenbelt, MD 20771 USA. EM johannes.g.staguhn@nasa.gov; dominic.benford@nasa.gov; harvey.moseley@nasa.gov RI Dwek, Eli/C-3995-2012; Benford, Dominic/D-4760-2012; Moseley, Harvey/D-5069-2012; Chuss, David/D-8281-2012; Wollack, Edward/D-4467-2012 OI Benford, Dominic/0000-0002-9884-4206; Wollack, Edward/0000-0002-7567-4451 FU NSF [0705185] FX THis work was sipported in party by NSF Grant AST 0705185 NR 8 TC 1 Z9 1 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 978-1-58381-714-8 J9 ASTR SOC P PY 2009 VL 417 BP 451 EP + PG 2 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BQL34 UT WOS:000281244000041 ER PT B AU Ghais, AF AF Ghais, Ahmad F. BE Sachdev, DK TI INMARSAT: A SUCCESS STORY SO SUCCESS STORIES IN SATELLITE SYSTEMS SE Library of Flight LA English DT Article; Book Chapter C1 [Ghais, Ahmad F.] INMARSAT, Engn & Operat, London, England. [Ghais, Ahmad F.] NASA, Washington, DC USA. RP Ghais, AF (reprint author), NASA, Washington, DC USA. NR 0 TC 1 Z9 1 U1 0 U2 0 PU AMER INST AERONAUTICS & ASTRONAUTICS PI RESTON PA 1801 ALEXANDER BELL DR, STE 500, RESTON, VA 20191-4344 USA BN 978-1-56347-966-3 J9 LIBR FLIGHT PY 2009 BP 95 EP + PG 26 WC Engineering, Aerospace SC Engineering GA BKF81 UT WOS:000267990500005 ER PT J AU Atlas, RM AF Atlas, Ronald M. GP Natl Res Council TI A SURVEY OF ATTITUDES AND ACTIONS ON DUAL USE RESEARCH IN THE LIFE SCIENCES A Collaborative Effort of the National Research Council and the American Association for the Advancement of Science Summary SO SURVEY OF ATTITUDES AND ACTIONS ON DUAL USE RESEARCH IN THE LIFE SCIENCES: A COLLABORATIVE EFFORT OF THE NATIONAL RESEARCH COUNCIL AND THE AMERICAN ASSOCIATION FOR THE ADVANCEMENT OF SCIENCE LA English DT Editorial Material; Book Chapter ID BIOLOGICAL WEAPONS; ETHICAL-ISSUES; SCIENTIFIC-RESEARCH; RESEARCH NORMS; 1918 FLU; VIRUS; GENETICS; CODES; INDUSTRY; FACULTY C1 [Atlas, Ronald M.] Univ Louisville, Biol & Publ Hlth, Louisville, KY 40292 USA. [Atlas, Ronald M.] Univ Louisville, Ctr Hlth Hazards Preparedness, Louisville, KY 40292 USA. [Atlas, Ronald M.] NASA, Planetary Protect Board, Washington, DC USA. [Atlas, Ronald M.] Wellcome Trust Infect Immunol & Populat Hlth Stra, Baltimore, MD USA. [Atlas, Ronald M.] ASM Task Force Biodef, Boston, MA USA. [Atlas, Ronald M.] ASM, Madison, WI USA. [Atlas, Ronald M.] NIH, Recombinant DNA Advisory Comm, Baltimore, MD USA. [Atlas, Ronald M.] Dept Homeland Secur Sci & Technol Advisory Comm, Oslo, Norway. [Atlas, Ronald M.] Fed Bur Invest Sci Working Grp Bioforens, London, England. RP Atlas, RM (reprint author), Univ Louisville, Biol & Publ Hlth, Louisville, KY 40292 USA. NR 168 TC 1 Z9 1 U1 0 U2 0 PU NATL ACADEMIES PRESS PI WASHINGTON PA 2101 CONSTITUTION AVE, WASHINGTON, DC 20418 USA BN 978-0-309-12510-9 PY 2009 BP 1 EP + PG 20 WC Education & Educational Research SC Education & Educational Research GA BC4IZ UT WOS:000352554100002 ER PT J AU Atlas, RM AF Atlas, Ronald M. GP Natl Res Council TI A SURVEY OF ATTITUDES AND ACTIONS ON DUAL USE RESEARCH IN THE LIFE SCIENCES A Collaborative Effort of the National Research Council and the American Association for the Advancement of Science Preface and Acknowledgments SO SURVEY OF ATTITUDES AND ACTIONS ON DUAL USE RESEARCH IN THE LIFE SCIENCES: A COLLABORATIVE EFFORT OF THE NATIONAL RESEARCH COUNCIL AND THE AMERICAN ASSOCIATION FOR THE ADVANCEMENT OF SCIENCE LA English DT Editorial Material; Book Chapter C1 [Atlas, Ronald M.] Univ Louisville, Biol & Publ Hlth, Louisville, KY 40292 USA. [Atlas, Ronald M.] Univ Louisville, Ctr Hlth Hazards Preparedness, Louisville, KY 40292 USA. [Atlas, Ronald M.] NASA, Planetary Protect Board, Washington, DC USA. [Atlas, Ronald M.] Wellcome Trust Infect Immunol & Populat Hlth Stra, Baltimore, MD USA. [Atlas, Ronald M.] ASM Task Force Biodef, Boston, MA USA. [Atlas, Ronald M.] ASM, Madison, WI USA. [Atlas, Ronald M.] NIH, Recombinant DNA Advisory Comm, Baltimore, MD USA. [Atlas, Ronald M.] Dept Homeland Secur Sci & Technol Advisory Comm, Oslo, Norway. [Atlas, Ronald M.] Fed Bur Invest Sci Working Grp Bioforens, London, England. RP Atlas, RM (reprint author), Univ Louisville, Biol & Publ Hlth, Louisville, KY 40292 USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU NATL ACADEMIES PRESS PI WASHINGTON PA 2101 CONSTITUTION AVE, WASHINGTON, DC 20418 USA BN 978-0-309-12510-9 PY 2009 BP VII EP IX PG 3 WC Education & Educational Research SC Education & Educational Research GA BC4IZ UT WOS:000352554100001 ER PT J AU Atlas, RM AF Atlas, Ronald M. GP Natl Res Council TI A SURVEY OF ATTITUDES AND ACTIONS ON DUAL USE RESEARCH IN THE LIFE SCIENCES A Collaborative Effort of the National Research Council and the American Association for the Advancement of Science Overview SO SURVEY OF ATTITUDES AND ACTIONS ON DUAL USE RESEARCH IN THE LIFE SCIENCES: A COLLABORATIVE EFFORT OF THE NATIONAL RESEARCH COUNCIL AND THE AMERICAN ASSOCIATION FOR THE ADVANCEMENT OF SCIENCE LA English DT Editorial Material; Book Chapter C1 [Atlas, Ronald M.] Univ Louisville, Biol & Publ Hlth, Louisville, KY 40292 USA. [Atlas, Ronald M.] Univ Louisville, Ctr Hlth Hazards Preparedness, Louisville, KY 40292 USA. [Atlas, Ronald M.] NASA, Planetary Protect Board, Washington, DC USA. [Atlas, Ronald M.] Wellcome Trust Infect Immunol & Populat Hlth Stra, Baltimore, MD USA. [Atlas, Ronald M.] ASM Task Force Biodef, Boston, MA USA. [Atlas, Ronald M.] ASM, Madison, WI USA. [Atlas, Ronald M.] NIH, Recombinant DNA Advisory Comm, Baltimore, MD USA. [Atlas, Ronald M.] Dept Homeland Secur Sci & Technol Advisory Comm, Oslo, Norway. [Atlas, Ronald M.] Fed Bur Invest Sci Working Grp Bioforens, London, England. RP Atlas, RM (reprint author), Univ Louisville, Biol & Publ Hlth, Louisville, KY 40292 USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU NATL ACADEMIES PRESS PI WASHINGTON PA 2101 CONSTITUTION AVE, WASHINGTON, DC 20418 USA BN 978-0-309-12510-9 PY 2009 BP 11 EP 41 PG 31 WC Education & Educational Research SC Education & Educational Research GA BC4IZ UT WOS:000352554100003 ER PT J AU Atlas, RM AF Atlas, Ronald M. GP Natl Res Council TI Approach SO SURVEY OF ATTITUDES AND ACTIONS ON DUAL USE RESEARCH IN THE LIFE SCIENCES: A COLLABORATIVE EFFORT OF THE NATIONAL RESEARCH COUNCIL AND THE AMERICAN ASSOCIATION FOR THE ADVANCEMENT OF SCIENCE LA English DT Article; Book Chapter C1 [Atlas, Ronald M.] Univ Louisville, Biol & Publ Hlth, Louisville, KY 40292 USA. [Atlas, Ronald M.] Univ Louisville, Ctr Hlth Hazards Preparedness, Louisville, KY 40292 USA. [Atlas, Ronald M.] NASA, Planetary Protect Board, Washington, DC USA. [Atlas, Ronald M.] Wellcome Trust Infect Immunol & Populat Hlth Stra, Baltimore, MD USA. [Atlas, Ronald M.] ASM Task Force Biodef, Boston, MA USA. [Atlas, Ronald M.] ASM, Madison, WI USA. [Atlas, Ronald M.] NIH, Recombinant DNA Advisory Comm, Baltimore, MD USA. [Atlas, Ronald M.] Dept Homeland Secur Sci & Technol Advisory Comm, Oslo, Norway. [Atlas, Ronald M.] Fed Bur Invest Sci Working Grp Bioforens, London, England. RP Atlas, RM (reprint author), Univ Louisville, Biol & Publ Hlth, Louisville, KY 40292 USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU NATL ACADEMIES PRESS PI WASHINGTON PA 2101 CONSTITUTION AVE, WASHINGTON, DC 20418 USA BN 978-0-309-12510-9 PY 2009 BP 43 EP 61 PG 19 WC Education & Educational Research SC Education & Educational Research GA BC4IZ UT WOS:000352554100004 ER PT J AU Atlas, RM AF Atlas, Ronald M. GP Natl Res Council TI Results of the Survey SO SURVEY OF ATTITUDES AND ACTIONS ON DUAL USE RESEARCH IN THE LIFE SCIENCES: A COLLABORATIVE EFFORT OF THE NATIONAL RESEARCH COUNCIL AND THE AMERICAN ASSOCIATION FOR THE ADVANCEMENT OF SCIENCE LA English DT Article; Book Chapter C1 [Atlas, Ronald M.] Univ Louisville, Biol & Publ Hlth, Louisville, KY 40292 USA. [Atlas, Ronald M.] Univ Louisville, Ctr Hlth Hazards Preparedness, Louisville, KY 40292 USA. [Atlas, Ronald M.] NASA, Planetary Protect Board, Washington, DC USA. [Atlas, Ronald M.] Wellcome Trust Infect Immunol & Populat Hlth Stra, Baltimore, MD USA. [Atlas, Ronald M.] ASM Task Force Biodef, Boston, MA USA. [Atlas, Ronald M.] ASM, Madison, WI USA. [Atlas, Ronald M.] NIH, Recombinant DNA Advisory Comm, Baltimore, MD USA. [Atlas, Ronald M.] Dept Homeland Secur Sci & Technol Advisory Comm, Oslo, Norway. [Atlas, Ronald M.] Fed Bur Invest Sci Working Grp Bioforens, London, England. RP Atlas, RM (reprint author), Univ Louisville, Biol & Publ Hlth, Louisville, KY 40292 USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU NATL ACADEMIES PRESS PI WASHINGTON PA 2101 CONSTITUTION AVE, WASHINGTON, DC 20418 USA BN 978-0-309-12510-9 PY 2009 BP 63 EP 113 PG 51 WC Education & Educational Research SC Education & Educational Research GA BC4IZ UT WOS:000352554100005 ER PT J AU Atlas, RM AF Atlas, Ronald M. GP Natl Res Council TI A SURVEY OF ATTITUDES AND ACTIONS ON DUAL USE RESEARCH IN THE LIFE SCIENCES A Collaborative Effort of the National Research Council and the American Association for the Advancement of Science Conclusions and Recommendations SO SURVEY OF ATTITUDES AND ACTIONS ON DUAL USE RESEARCH IN THE LIFE SCIENCES: A COLLABORATIVE EFFORT OF THE NATIONAL RESEARCH COUNCIL AND THE AMERICAN ASSOCIATION FOR THE ADVANCEMENT OF SCIENCE LA English DT Editorial Material; Book Chapter C1 [Atlas, Ronald M.] Univ Louisville, Biol & Publ Hlth, Louisville, KY 40292 USA. [Atlas, Ronald M.] Univ Louisville, Ctr Hlth Hazards Preparedness, Louisville, KY 40292 USA. [Atlas, Ronald M.] NASA, Planetary Protect Board, Washington, DC USA. [Atlas, Ronald M.] Wellcome Trust Infect Immunol & Populat Hlth Stra, Baltimore, MD USA. [Atlas, Ronald M.] ASM Task Force Biodef, Boston, MA USA. [Atlas, Ronald M.] ASM, Madison, WI USA. [Atlas, Ronald M.] NIH, Recombinant DNA Advisory Comm, Baltimore, MD USA. [Atlas, Ronald M.] Dept Homeland Secur Sci & Technol Advisory Comm, Oslo, Norway. [Atlas, Ronald M.] Fed Bur Invest Sci Working Grp Bioforens, London, England. RP Atlas, RM (reprint author), Univ Louisville, Biol & Publ Hlth, Louisville, KY 40292 USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU NATL ACADEMIES PRESS PI WASHINGTON PA 2101 CONSTITUTION AVE, WASHINGTON, DC 20418 USA BN 978-0-309-12510-9 PY 2009 BP 115 EP 122 PG 8 WC Education & Educational Research SC Education & Educational Research GA BC4IZ UT WOS:000352554100006 ER PT J AU Feidas, H Kokolatos, G Negri, A Manyin, M Chrysoulakis, N Kamarianakis, Y AF Feidas, H. Kokolatos, G. Negri, A. Manyin, M. Chrysoulakis, N. Kamarianakis, Y. TI Validation of an infrared-based satellite algorithm to estimate accumulated rainfall over the Mediterranean basin SO THEORETICAL AND APPLIED CLIMATOLOGY LA English DT Article ID PRECIPITATION ESTIMATION; RETRIEVAL ALGORITHMS; CLOUD; IMAGERY; MICROWAVE; PENINSULA; RADAR AB The potential of an infrared-based satellite rainfall algorithm, the well-known Convective-Stratiform technique (CST), to estimate accumulated rainfall in the Mediterranean basin is tested. The CST, calibrated by coincident, physically retrieved rainfall rates from the Tropical Rainfall Measuring Mission (TRMM) Precipitation Radar (PR), is applied over the central-eastern Mediterranean region for the twelve-month period September 2004-August 2005. Estimates from this technique are verified over a 1A degrees x1A degrees gridded precipitation dataset, based on rain gauge data only, for different time scales (monthly, seasonal and annual). The comparisons between satellite-derived precipitation estimates and validation data provide a high correlation coefficient (0.88) and low biases only for the summer season. In contrast, the comparison statistics for winter demonstrate the shortcomings of the CST algorithm in reproducing adequately the precipitation field in the mid-latitudes during this season. Although the correlations for spring and annual precipitation are relatively high (0.76 and 0.73, respectively), a strong positive bias exists. Rainfall variability is less adequately reproduced for the autumn, but the errors are within an acceptable range. A comparison test conducted in the different climate zones of the study area indicated that the calibrated CST performs better in the sub-tropical deserts and steppes of northern Africa and in humid, continental climates. Mediterranean climates produce higher correlations for autumn, summer and spring precipitation, whereas humid sub-tropical climates present the lowest correlation coefficients. Finally, the potential of the CST technique in climatic studies was demonstrated by studying the diurnal variability of precipitation at high spatial and temporal resolutions. C1 [Feidas, H.] Aristotle Univ Thessaloniki, Dept Geol, Div Meteorology Climatol, Thessaloniki 54124, Greece. [Kokolatos, G.] Univ Aegean, Dept Geog, Mitilini, Greece. [Negri, A.] NASA, Goddard Space Flight Ctr, Atmospheres Lab, Greenbelt, MD 20771 USA. [Manyin, M.] Sci Syst & Applicat Inc, Lanham, MD USA. [Chrysoulakis, N.; Kamarianakis, Y.] Fdn Res & Technol Hellas, Reg Anal Div, Inst Appl & Computat Math, Iraklion, Crete, Greece. RP Feidas, H (reprint author), Aristotle Univ Thessaloniki, Dept Geol, Div Meteorology Climatol, Thessaloniki 54124, Greece. EM xfeidas@geo.aegean.gr RI Manyin, Michael/D-7756-2012 FU Ministry of Development of Greece. FX This work was conducted as part of the SATERM (A Satellite Technique for Estimating Rainfall over the Mediterranean basin) project funded by the Project "Competitiveness'', Action 4.3.6.1d "Cooperation with R&T institutions in non-European countries'' of the General Secretary of Research and Technology, Ministry of Development of Greece. NR 50 TC 11 Z9 12 U1 0 U2 1 PU SPRINGER WIEN PI WIEN PA SACHSENPLATZ 4-6, PO BOX 89, A-1201 WIEN, AUSTRIA SN 0177-798X J9 THEOR APPL CLIMATOL JI Theor. Appl. Climatol. PD JAN PY 2009 VL 95 IS 1-2 BP 91 EP 109 DI 10.1007/s00704-007-0360-y PG 19 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 396FI UT WOS:000262577200008 ER PT B AU Lunine, J Choukroun, M Stevenson, D Tobie, G AF Lunine, Jonathan Choukroun, Mathieu Stevenson, David Tobie, Gabriel BE Brown, RH Lebreton, JP Waite, JH TI The Origin and Evolution of Titan SO TITAN FROM CASSINI-HUYGENS LA English DT Article; Book Chapter ID GIANT PLANET FORMATION; LARGE ICY SATELLITES; OUTER SOLAR-SYSTEM; PROTOPLANETARY DISKS; GALILEAN SATELLITES; INTERNAL STRUCTURE; THERMAL EVOLUTION; HIGH-PRESSURE; THERMODYNAMIC PROPERTIES; ATMOSPHERIC METHANE AB Titan was formed as a regular satellite in a disk that was the outgrowth of the formation of Saturn itself. Unlike the Jovian system, Titan is alone in terms of its size and mass, not part of a system gradational in density and hence rock abundance, perhaps reflecting a smaller disk and greater importance of stochastic events during satellite assembly. Accretional heating of Titan was enough to melt an outer layer of water (a water "magma ocean") and sustain for a short period an environment in which exposed water or water-ammonia liquid was in contact with organic molecules. Initial warm surface conditions are supported by direct samplings of Titan's atmosphere by the mass spectrometers on board Cassini and Huygens, which provide circumstantial evidence that ammonia (NH(3)) is the primordial Source of Titan's atmospheric molecular nitrogen. Ammonia can be extracted from the liquid phase only if the surface temperature is above the melting point of the mixture, thus implying warm accretion. The carbon isotopic ratio (13)C/(12)C in hydrocarbon molecules measured by the GCMS on Huygens reflects a bulk carbon inventory that did not participate in the massive escape phase of the ancient post-accretional atmosphere, in contrast to nitrogen, whose isotopic ratio (15)N/(14)N is modestly enhanced and thus suggests escape, though how much depends on the mechanism. The presence of a significant amount of the (40)K decay daughter (40)Ar strongly suggests that internal outgassing of volatiles, including methane and argon, has occurred through Titan's history. Different models of the thermal and structure evolution of Titan's interior have been proposed to explain the persistence of methane at the surface over the age of the solar system (of order 100 times the lifetime of the known reservoirs of methane in the surface and atmosphere), and a modest dearth of impact craters consistent with a surface age of about a billion years. A first post-Cassini-Huygens model suggests that the formation of thin crust enriched in methane clathrate, owing to interactions between the primordial ocean and the primitive atmosphere as well as release of volatiles from the deep interior, could have delayed the crystallization of the internal ocean, favoring outgassing of methane at different epochs. C1 [Lunine, Jonathan] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA. [Choukroun, Mathieu] NASA, Jet Prop Lab, Pasadena, CA 91109 USA. [Stevenson, David] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. [Tobie, Gabriel] Univ Nantes, Lab Planetol & Geodynam, F-44312 Nantes 3, France. RP Lunine, J (reprint author), Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA. EM jlunine@lpl.arizona.edu RI Choukroun, Mathieu/F-3146-2017 OI Choukroun, Mathieu/0000-0001-7447-9139 NR 148 TC 18 Z9 18 U1 0 U2 5 PU SPRINGER PI DORDRECHT PA PO BOX 17, 3300 AA DORDRECHT, NETHERLANDS BN 978-1-4020-9214-5 PY 2009 BP 35 EP 59 DI 10.1007/978-1-4020-9215-2_3 PG 25 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BMN07 UT WOS:000272894300003 ER PT B AU Sotin, C Mitri, G Rappaport, N Schubert, G Stevenson, D AF Sotin, Christophe Mitri, Giuseppe Rappaport, Nicole Schubert, Gerald Stevenson, David BE Brown, RH Lebreton, JP Waite, JH TI Titan's Interior Structure SO TITAN FROM CASSINI-HUYGENS LA English DT Article; Book Chapter ID LARGE VISCOSITY VARIATIONS; LARGE ICY SATELLITES; INTERNAL STRUCTURE; THERMAL-CONVECTION; HUYGENS PROBE; PHYSICAL-CHARACTERISTICS; GALILEAN SATELLITES; TIDAL DISSIPATION; ATMOSPHERE; SHELL AB The goal of this chapter is to give a description of Titan's interior that is consistent with the new constraints provided by the Cassini mission. As the Cassini mission proceeds into its first extended phase, the data obtained during the nominal mission suggest that Titan is at least partially differentiated. An ocean would be present some tens of kilometers below the surface. By comparison with the Galilean icy satellites Ganymede and Callisto, Titan would be composed of a metal/silicate rich core and a H2O rich outer layer. These conclusions are drawn from the interpretation of the gravity data, the geological data and the presence of a Schumann resonance which has been inferred from the measurement of electric signals during the descent of the Huygens probe into Titan's atmosphere. Titan's high eccentricity implies that the interior has not been very dissipative, there is little tidal heating available for internal dynamics, and the ice layer is cold, which can be achieved if the ocean under the ice layer contains ammonia. This paper also describes observations and interpretations which seem difficult to reconcile with our present understanding of Titan's interior structure and evolution such as the shape of the planet or the obliquity. The last part of the chapter describes heat transfer models which suggest that the lower part of the ice crust could be convective. The NH3-H2O phase diagram indicates that the ocean is decoupled from the silicate-rich core by a layer of high-pressure ices. However, the interior model is largely uncertain because the interpretation of the data is still debated at present time. The additional information that will be acquired during the Cassini Solstice Mission should allow us to answer some of the questions. C1 [Sotin, Christophe; Mitri, Giuseppe; Rappaport, Nicole] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Schubert, Gerald] Univ Calif Los Angeles, Los Angeles, CA USA. RP Sotin, C (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr,Mail Stop 183-301, Pasadena, CA 91109 USA. EM christophe.sotin@jpl.nasa.gov NR 58 TC 16 Z9 16 U1 0 U2 1 PU SPRINGER PI DORDRECHT PA PO BOX 17, 3300 AA DORDRECHT, NETHERLANDS BN 978-1-4020-9214-5 PY 2009 BP 61 EP 73 DI 10.1007/978-1-4020-9215-2_4 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BMN07 UT WOS:000272894300004 ER PT B AU Jaumann, R Kirk, RL Lorenz, RD Lopes, RMC Stofan, E Turtle, EP Keller, HU Wood, CA Sotin, C Soderblom, LA Tomasko, MG AF Jaumann, Ralf Kirk, Randolph L. Lorenz, Ralph D. Lopes, Rosaly M. C. Stofan, Ellen Turtle, Elizabeth P. Keller, Horst Uwe Wood, Charles A. Sotin, Christophe Soderblom, Laurence A. Tomasko, Martin G. BE Brown, RH Lebreton, JP Waite, JH TI Geology and Surface Processes on Titan SO TITAN FROM CASSINI-HUYGENS LA English DT Article; Book Chapter ID HUYGENS LANDING SITE; BIDIRECTIONAL REFLECTANCE SPECTROSCOPY; DESCENT IMAGER/SPECTRAL RADIOMETER; CASSINI RADAR OBSERVATIONS; MAPPING SPECTROMETER VIMS; ADAPTIVE OPTICS; TIDAL DISSIPATION; IMAGING SCIENCE; SATURN SYSTEM; MU-M AB The surface of Titan has been revealed globally, if incompletely, by Cassini observations at infrared and radar wavelengths as well as locally by the instruments on the Huygens probe. Extended dune fields, lakes, mountainous terrain, dendritic erosion patterns and erosional remnants indicate dynamic surface processes. Valleys, small-scale gullies and rounded cobbles such as those observed at the Huygens landing site require erosion by energetic flow of a liquid. There is strong evidence that liquid hydrocarbons are ponded on the surface in high-latitude lakes, predominantly, but not exclusively, at high northern latitudes. A variety of features including extensive flows and caldera-like constructs are interpreted to be cryovolcanic in origin. Chains and isolated blocks of rugged terrain rising from smoother areas are best described as mountains and might be related to tectonic processes. Finally, impact craters are observed but their small numbers indicate that the crater retention age is very young overall. In general, Titan exhibits a geologically active surface indicating significant endogenic and exogenic processes, with diverse geophysical and atmospheric processes reminiscent of those on Earth. C1 [Jaumann, Ralf] DLR, Inst Planetary Res, D-12489 Berlin, Germany. [Jaumann, Ralf] Free Univ Berlin, Inst Geol Sci, D-12249 Berlin, Germany. [Kirk, Randolph L.; Soderblom, Laurence A.] US Geol Survey, Flagstaff, AZ 86001 USA. [Lorenz, Ralph D.; Turtle, Elizabeth P.] Johns Hopkins Univ, Appl Phys Lab, Dept Space, Laurel, MD 20723 USA. [Lopes, Rosaly M. C.; Sotin, Christophe] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Stofan, Ellen] Proxemy Res, Rectortown, VA 20140 USA. [Keller, Horst Uwe] Max Planck Inst Solar Syst Res, Katlenburg Lindau, Germany. [Wood, Charles A.] Planetary Sci Inst, Tucson, AZ 85719 USA. [Tomasko, Martin G.] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA. RP Jaumann, R (reprint author), DLR, Inst Planetary Res, Rutherfordstr 2, D-12489 Berlin, Germany. EM ralf.jaumann@dlr.de RI Turtle, Elizabeth/K-8673-2012; Lorenz, Ralph/B-8759-2016 OI Turtle, Elizabeth/0000-0003-1423-5751; Lorenz, Ralph/0000-0001-8528-4644 NR 230 TC 18 Z9 18 U1 0 U2 5 PU SPRINGER PI DORDRECHT PA PO BOX 17, 3300 AA DORDRECHT, NETHERLANDS BN 978-1-4020-9214-5 PY 2009 BP 75 EP 140 DI 10.1007/978-1-4020-9215-2_5 PG 66 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BMN07 UT WOS:000272894300005 ER PT B AU Soderblom, LA Barnes, JW Brown, RH Clark, RN Janssen, MA McCord, TB Niemann, HB Tomasko, MG AF Soderblom, L. A. Barnes, J. W. Brown, R. H. Clark, R. N. Janssen, M. A. McCord, T. B. Niemann, H. B. Tomasko, M. G. BE Brown, RH Lebreton, JP Waite, JH TI Composition of Titan's Surface SO TITAN FROM CASSINI-HUYGENS LA English DT Article; Book Chapter ID HUYGENS LANDING SITE; DESCENT IMAGER/SPECTRAL RADIOMETER; MAPPING SPECTROMETER VIMS; COMPLEX ORGANIC-MATTER; CASSINI RADAR; ICY SATELLITES; MU-M; DIELECTRIC-PROPERTIES; INFRARED OBSERVATIONS; REFLECTANCE SPECTRA AB The Huygens Probe returned the first in situ data on Titan's surface composition in January 2005. Although Huygens landed on a dry plain, the Gas Chromatograph Mass Spectrometer (GCMS) showed evidence of methane moisture in the near subsurface suggesting methane precipitation at some time in the past. Heavier organic molecules were not found to be abundant in the atmosphere or at the surface, but the GCMS surface results did show ethane to be present and tentatively identified cyanogen, benzene, and carbon dioxide. During descent, aerosol particles were processed with the Aerosol Collector and Pyroliser; results suggested that the aerosols contain both nitrites and hydrocarbons. The Descent Imager/Spectral Radiometer (DISR also carried by the probe) measured the visible and near-infrared spectral reflectance of the dark plain surface at the landing site. Those data suggest a mixture of water ice, tholin-like materials, and dark neutral material with a blue slope in the near infrared; identification of water ice is suggested but inconclusive. Most remarkably DISR did not detect spectral features, beyond those for methane, for a wide range of spectrally active hydrocarbon and nitrile compounds that had been expected to be present on the surface. C1 [Soderblom, L. A.] US Geol Survey, Astrogeol Team, Flagstaff, AZ 86004 USA. [Barnes, J. W.] Univ Idaho, Moscow, ID 83844 USA. [Brown, R. H.; Tomasko, M. G.] Univ Arizona, Tucson, AZ 85721 USA. [Clark, R. N.] US Geol Survey, Denver, CO 80225 USA. [Janssen, M. A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [McCord, T. B.] Bear Fight Ctr, Winthrop, WA 98862 USA. [Niemann, H. B.] NASA, Greenbelt, MD 20771 USA. RP Soderblom, LA (reprint author), US Geol Survey, Astrogeol Team, Flagstaff, AZ 86004 USA. EM lsoderblom@usgs.gov NR 128 TC 8 Z9 8 U1 2 U2 3 PU SPRINGER PI DORDRECHT PA PO BOX 17, 3300 AA DORDRECHT, NETHERLANDS BN 978-1-4020-9214-5 PY 2009 BP 141 EP 175 DI 10.1007/978-1-4020-9215-2_6 PG 35 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BMN07 UT WOS:000272894300006 ER PT B AU Waite, JH Young, DT Westlake, JH Lunine, JI McKay, CP Lewis, WS AF Waite, J. H., Jr. Young, D. T. Westlake, J. H. Lunine, J. I. McKay, C. P. Lewis, W. S. BE Brown, RH Lebreton, JP Waite, JH TI High-Altitude Production of Titan's Aerosols SO TITAN FROM CASSINI-HUYGENS LA English DT Article; Book Chapter ID UPPER-ATMOSPHERE; HAZE FORMATION; COUPLING PHOTOCHEMISTRY; INFRARED OBSERVATIONS; ORGANIC-CHEMISTRY; SATURNIAN SYSTEM; MODEL; VOYAGER-1; THOLIN; ION AB Measurements with the Cassini Ion and Neutral Mass Spectrometer (INMS) and two Cassini Plasma Spectrometer (CAPS) sensors, the Ion beam Spectrometer (IBS) and the Electron Spectrometer (ELS), have revealed the presence of a significant population of heavy hydrocarbon and nitrile species well above the homopause, with masses as large as several thousand Daltons (Da). The INMS ion and neutral spectra cover the mass range 1-100 Da. The IBS has measured positive ions up to 350 Da, while the ELS has detected concentrations of negative ions as high as 20% of the total negatively charged ionosphere component extending to over 13,000 Da. These measurements have motivated the development of new atmospheric models and have significant implications for our knowledge and understanding of Titan's haze layers. C1 [Waite, J. H., Jr.; Young, D. T.; Westlake, J. H.; Lewis, W. S.] SW Res Inst, San Antonio, TX 78228 USA. [Waite, J. H., Jr.; Westlake, J. H.] Univ Texas San Antonio, San Antonio, TX 78249 USA. [Lunine, J. I.] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA. [McKay, C. P.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Waite, JH (reprint author), SW Res Inst, PO Drawer 28510, San Antonio, TX 78228 USA. EM hwaite@swri.edu RI Westlake, Joseph/G-2732-2015 OI Westlake, Joseph/0000-0003-0472-8640 NR 64 TC 11 Z9 11 U1 0 U2 4 PU SPRINGER PI DORDRECHT PA PO BOX 17, 3300 AA DORDRECHT, NETHERLANDS BN 978-1-4020-9214-5 PY 2009 BP 201 EP 214 DI 10.1007/978-1-4020-9215-2_8 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BMN07 UT WOS:000272894300008 ER PT B AU Raulin, F McKay, C Lunine, J Owen, T AF Raulin, F. McKay, C. Lunine, J. Owen, T. BE Brown, RH Lebreton, JP Waite, JH TI Titan's Astrobiology SO TITAN FROM CASSINI-HUYGENS LA English DT Article; Book Chapter ID PHOTOCHEMICAL KINETICS UNCERTAINTIES; ATMOSPHERIC CHEMISTRY; HAZE FORMATION; ORGANIC HAZE; EARLY EARTH; PRIMITIVE EARTH; IN-SITU; COUPLING PHOTOCHEMISTRY; LABORATORY SIMULATIONS; HETEROGENEOUS REACTION AB This chapter describes the aspects of Saturn's moon Titan of astrobiological interest. Titan's prebiotic-like chemistry is reviewed, from the high atomosphere to the surface and subsurface, using the Cassini-Huygens data, with the help of theoretical modeling and experimental simulations. Similarities with and differences from the environment of the pre-biotic Earth are presented, and the lessons to be learned for Earth's organic chemical evolution on the prebiotic Earth discussed. The question of habitability and life on and in Titan is then considered, including the possibility of an exotic type of life that might exist in the liquid methane/ethane lakes. Finally. the relation between Titan and the destiny of life on Earth is discussed. C1 [Raulin, F.] Univ Paris, LISA, Paris 12, France. [Raulin, F.] Univ Paris, LISA, Paris 7, France. [McKay, C.] NASA Ames, Ames, IA USA. [Lunine, J.] Univ Arizona, LPL, Tucson, AZ USA. [Owen, T.] Univ Hawaii, Honolulu, HI 96822 USA. RP Raulin, F (reprint author), Univ Paris, LISA, Paris 12, France. EM raulin@lisa.univ-paris12.fr NR 133 TC 14 Z9 15 U1 2 U2 11 PU SPRINGER PI DORDRECHT PA PO BOX 17, 3300 AA DORDRECHT, NETHERLANDS BN 978-1-4020-9214-5 PY 2009 BP 215 EP 233 DI 10.1007/978-1-4020-9215-2_9 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BMN07 UT WOS:000272894300009 ER PT B AU Strobel, DF Atreya, SK Bezard, B Ferri, F Flasar, FM Fulchignoni, M Lellouch, E Muller-Wodarg, I AF Strobel, Darrell F. Atreya, Sushil K. Bezard, Bruno Ferri, Francesca Flasar, F. Michael Fulchignoni, Marcello Lellouch, Emmanuel Mueller-Wodarg, Ingo BE Brown, RH Lebreton, JP Waite, JH TI Atmospheric Structure and Composition SO TITAN FROM CASSINI-HUYGENS LA English DT Article; Book Chapter ID TITANS UPPER-ATMOSPHERE; HYDRODYNAMICALLY ESCAPING ATMOSPHERE; VOYAGER-1 RADIO-OCCULTATION; ISOTOPIC-RATIOS; CASSINI CIRS; STRATOSPHERIC TEMPERATURE; HETEROGENEOUS REACTION; LATITUDINAL VARIATIONS; INFRARED OBSERVATIONS; HYPOTHESIZED OCEAN AB Titan's atmosphere is predominantly N-2 with CH4 the next most abundant molecule. It has a mole fraction of 0.05 just above the surface decreasing to 0.014 in the stratosphere. Above the homopause (similar to 800-850 km), it increases to 0.12 at the exobase. The third abundant molecule is H-2 with a tropospheric mole fraction of 0.001 increasing to 0.004 at similar to 1000 km and similar to 0.02 at the exobase (similar to 1500-1600 km). This chapter reviews the various measurements acquired by the Voyager flybys, Huygens Probe, orbiting Cassini spacecraft. ground-based and orbiting telescopes of the large suite of hydrocarbons, nitriles, other nitrogen and also oxygen bearing compounds. Titan possesses a mostly stable troposphere with a well defined tropopause (T similar to 70 K at similar to 44 km) and a lower stratosphere with a high static stability, which is extremely cold over the winter polar region (currently northern hemisphere) and warm over the summer pole. Remarkably in the middle stratosphere, the warmest temperatures occur at the equator and the largest meridional temperature gradients are found in the winter hemisphere. The stratopause from the summer pole to about 45 degrees N remains at a relatively constant pressure of 0.1 mbar/300 km and then it rises rapidly upward to similar to 0.01 mbar/400 km at the winter north pole, where it is the warmest region in the entire atmosphere. One possible interpretation of the Huygens Atmospheric Structure Instrument (HASI) temperature profile is that Titan's atmosphere is essentially isothermal similar to 170 K from 500-1100 km, with large amplitude thermal waves (10 K) superimposed. The existence and location of a well defined mesopause is an open question. The chemistry of Titan's atmosphere is driven by CH4 photolysis in the thermosphere and catalytic reactions in the stratosphere, and by N-2 dissociation due to both UV photons and energetic electrons. Ethane is the most abundant gas product and HCN is the dominant nitrile. The mixing ratios of all photochemical species, except C2H4, increase with altitude at equatorial and Southern latitudes, indicative of transport from a high-altitude source to a condensation sink in the lower stratosphere. Northward of 45 degrees N, most product compounds are enriched as a consequence of subsidence in the winter polar vortex, particularly for nitriles and more complex hydrocarbons than C2H6 and C2H2. North of 45 degrees N, most products have lower increases with attitude than at low latitudes. C1 [Strobel, Darrell F.] Johns Hopkins Univ, Baltimore, MD 21218 USA. [Atreya, Sushil K.] Univ Michigan, Ann Arbor, MI 48109 USA. [Bezard, Bruno; Fulchignoni, Marcello; Lellouch, Emmanuel] Observ Paris, LESIA, F-92195 Meudon, France. [Ferri, Francesca] Univ Padua, CISAS G Colombo, I-35131 Padua, Italy. [Flasar, F. Michael] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Mueller-Wodarg, Ingo] Univ London Imperial Coll Sci Technol & Med, Space & Atmospher Phys Grp, London SW7 2BW, England. RP Strobel, DF (reprint author), Johns Hopkins Univ, Baltimore, MD 21218 USA. EM strobel@jhu.edu; atreya@umich.edu; Bruno.Bezard@obspm.fr; francesca.ferri@unipd.it; f.m.flasar@nasa.gov; marcello.fulchignoni@obspm.fr; emmanuel.lellouch@obspm.fr; i.mueller-wodarg@imperial.ac.uk RI Flasar, F Michael/C-8509-2012 NR 104 TC 24 Z9 24 U1 0 U2 5 PU SPRINGER PI DORDRECHT PA PO BOX 17, 3300 AA DORDRECHT, NETHERLANDS BN 978-1-4020-9214-5 PY 2009 BP 235 EP 257 DI 10.1007/978-1-4020-9215-2_10 PG 23 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BMN07 UT WOS:000272894300010 ER PT B AU Tomasko, MG West, RA AF Tomasko, Martin G. West, Robert A. BE Brown, RH Lebreton, JP Waite, JH TI Aerosols in Titan's Atmosphere SO TITAN FROM CASSINI-HUYGENS LA English DT Article; Book Chapter ID IMAGER/SPECTRAL RADIOMETER DISR; NORTH POLAR STRATOSPHERE; GENERAL-CIRCULATION; AGGREGATE PARTICLES; MIDLATITUDE CLOUDS; OPTICAL-PROPERTIES; CONDENSATE CLOUDS; ORGANIC-CHEMISTRY; HYDROGEN-CYANIDE; HUYGENS PROBE AB Aerosols in Titan's atmosphere play important roles in the transfer of solar and thermal radiation, in Titan's heat balance, in forcing atmospheric dynamics, and as a sink for photochemical reactions. In this chapter we briefly summarize the history of our knowledge of their distribution and optical properties before concentrating in greater detail on current knowledge of their properties and roles in the physics and chemistry in Titan's atmosphere. We discuss the size, shape, optical properties, and the vertical distribution of Titan's aerosols. We discuss variations of the optical properties of the aerosols with wavelength, variations of the distribution of the aerosols over the disk of Titan, and the seasonal and long-term variations in structure. We discuss the visible and thermal opacity of the aerosols, and their roles in Titan's heat balance. We summarize the history and current state of laboratory simulations of these particles, and present our understanding of their formation and life cycles in one and two-dimensional microphysical models. We also discuss the presence, location, and variations in condensation clouds over Titan's disk. Finally, we indicate the prospects for further progress in understanding the origin, distribution, and properties of Titan's aerosols in the future. C1 [Tomasko, Martin G.] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA. [West, Robert A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Tomasko, MG (reprint author), Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA. EM mtomasko@lpl.arizona.edu NR 89 TC 10 Z9 10 U1 3 U2 3 PU SPRINGER PI DORDRECHT PA PO BOX 17, 3300 AA DORDRECHT, NETHERLANDS BN 978-1-4020-9214-5 PY 2009 BP 297 EP 321 DI 10.1007/978-1-4020-9215-2_12 PG 25 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BMN07 UT WOS:000272894300012 ER PT B AU Flasar, FM Baines, KH Bird, MK Tokano, T West, RA AF Flasar, F. M. Baines, K. H. Bird, M. K. Tokano, T. West, R. A. BE Brown, RH Lebreton, JP Waite, JH TI Atmospheric Dynamics and Meteorology SO TITAN FROM CASSINI-HUYGENS LA English DT Article; Book Chapter ID COMPOSITE INFRARED SPECTROMETER; VOYAGER-1 RADIO-OCCULTATION; TITANS MIDLATITUDE CLOUDS; GENERAL-CIRCULATION MODEL; HUYGENS PROBE; ZONAL WINDS; EQUATORIAL SUPERROTATION; TROPOSPHERIC CLOUDS; CASSINI RADAR; LATITUDINAL VARIATIONS AB Titan, after Venus, is the second example in the solar system of an atmosphere with a global cyclostrophic circulation, but in this case a circulation that has a strong seasonal modulation in the middle atmosphere. Direct measurement of Titan's winds., particularly observations tracking the Huygens probe at 10 degrees S, indicate that the zonal winds are mostly in the sense of the satellite's rotation. They generally increase with altitude and become cyclostrophic near 35 km above the surface. An exception to this is a sharp minimum centered near 75 km, where the wind velocity decreases to nearly zero. Zonal winds derived from temperatures retrieved from Cassini orbiter measurements, using the thermal wind equation, indicate a strong winter circumpolar vortex, with maximum winds of 190 m s(-1) at mid northern latitudes near 300 kin. Above this level, the vortex decays. Curiously, the stratospheric zonal winds and temperatures in both hemispheres are symmetric about a pole that is offset from the surface pole by similar to 4 degrees. The cause of this is not well understood, but it may reflect the response of a cyclostrophic circulation to the offset between the equator, where the distance to the rotation axis is Greatest, and the seasonally varying subsolar latitude. The mean meridional circulation can be inferred from the temperature field and the meridional distribution of organic molecules and condensates and hazes. Both the warm temperatures near 400 km and the enhanced concentration of several organic molecules suggest subsidence in the north-polar region during winter and early spring. Stratospheric condensates are localized at high northern latitudes, with a sharp cut-off near 50 degrees N. Titan's winter polar vortex appears to share many of the same characteristics of isolating high and low-latitude air masses as do the winter polar vortices on Earth that envelop the ozone holes. Global mapping of temperatures, winds, and composition in the troposphere, by contrast, is incomplete. The few suitable discrete clouds that have been found for tracking indicate smaller velocities than aloft, consistent with the Huygens measurements. Along the descent trajectory, the Huygens measurements indicate eastward zonal winds down to 7 km, where they shift westward, and then eastward again below 1 km down to the surface. The low-latitude dune fields seen in Cassini RADAR images have been interpreted as longitudinal dunes occurring in a mean eastward zonal wind. This is not like Earth, where the low-latitude winds are westward above the surface. Because the net zonal-mean time-averaged torque exerted by the surface on the atmosphere should vanish, there must be westward flow over part of the surface; the question is where and when. The meridional contrast in tropospheric temperatures, deduced from radio occultations at low, mid, and high latitudes, is small, similar to 5 K at the tropopause and similar to 3 K at the surface. This implies efficient heat transport, probably by axisymmetric meridional circulations. The effect of the methane "hydrological" cycle on the atmospheric circulation is not well constrained by existing measurements. Understanding the nature of the surface-atmosphere coupling will be critical to elucidating the atmospheric transports of momentum, heat, and volatiles. C1 [Flasar, F. M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Baines, K. H.; West, R. A.] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. [Bird, M. K.] Univ Bonn, D-5300 Bonn, Germany. [Tokano, T.] Univ Cologne, D-5000 Cologne 41, Germany. RP Flasar, FM (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. EM f.m.flasar@nasa.gov RI Flasar, F Michael/C-8509-2012 NR 141 TC 8 Z9 8 U1 0 U2 3 PU SPRINGER PI DORDRECHT PA PO BOX 17, 3300 AA DORDRECHT, NETHERLANDS BN 978-1-4020-9214-5 PY 2009 BP 323 EP 352 DI 10.1007/978-1-4020-9215-2_13 PG 30 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BMN07 UT WOS:000272894300013 ER PT B AU Lorenz, RD Brown, ME Flasar, FM AF Lorenz, Ralph D. Brown, Michael E. Flasar, F. Michael BE Brown, RH Lebreton, JP Waite, JH TI Seasonal Change on Titan SO TITAN FROM CASSINI-HUYGENS LA English DT Article; Book Chapter ID HUBBLE-SPACE-TELESCOPE; ZONAL WINDS; GENERAL-CIRCULATION; MIDLATITUDE CLOUDS; CASSINI/CIRS DATA; LOWER ATMOSPHERE; SATURN SYSTEM; SURFACE; MODEL; STRATOSPHERE AB Titan displays seasonal changes in the distribution of gas and hazes in its atmosphere, in the character of its methane clouds, and in its temperatures and winds. While Cassini has observed some of these changes in detail, some are observable from Earth, and the period of most rapid change may be just about to begin in the years after equinox. C1 [Lorenz, Ralph D.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD USA. [Brown, Michael E.] CALTECH, Pasadena, CA 91125 USA. [Flasar, F. Michael] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Lorenz, RD (reprint author), Johns Hopkins Univ, Appl Phys Lab, Laurel, MD USA. EM ralph.lorenz@jhuapl.edu RI Flasar, F Michael/C-8509-2012; Lorenz, Ralph/B-8759-2016 OI Lorenz, Ralph/0000-0001-8528-4644 NR 108 TC 7 Z9 7 U1 0 U2 2 PU SPRINGER PI DORDRECHT PA PO BOX 17, 3300 AA DORDRECHT, NETHERLANDS BN 978-1-4020-9214-5 PY 2009 BP 353 EP 372 DI 10.1007/978-1-4020-9215-2_14 PG 20 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BMN07 UT WOS:000272894300014 ER PT B AU Johnson, RE Tucker, OJ Michael, M Sittler, EC Smith, HT Young, DT Waite, JH AF Johnson, R. E. Tucker, O. J. Michael, M. Sittler, E. C. Smith, H. T. Young, D. T. Waite, J. H. BE Brown, RH Lebreton, JP Waite, JH TI Mass Loss Processes in Titan's Upper Atmosphere SO TITAN FROM CASSINI-HUYGENS LA English DT Article; Book Chapter ID HYDRODYNAMICALLY ESCAPING ATMOSPHERE; PICK-UP IONS; SATURNS MAGNETOSPHERE; ENCELADUS; NITROGEN; PLASMA; SPECTROMETER; EVOLUTION; VOYAGER-1; EXOSPHERE AB Although Titan's atmospheric column density is about ten times that of the Earth's, its measured N-15/N-14 ratio suggests that considerable escape has occurred or that Titan's original material had a ratio closer to that of cometary materials. A number of active escape processes have been proposed: thermal escape, chemical-induced escape, slow hydrodynamic escape, pick-up ion loss, ionospheric outflow and plasma-ion-induced atmospheric sputtering. These loss processes and relevant simulations are reviewed in light of recent Cassini data. Analysis of Cassini data collected in Titan's thermosphere and corona indicate that thermal loss of hydrogen occurs at a rate comparable to pre-Cassini estimates. This escape of hydrogen is accompanied by a significant loss of methane due to formation and precipitation of hydrocarbons (similar to 2 x 10(29) amu/s). However, there is much less agreement on the rates for the escape of methane and nitrogen. Recent estimates, similar to 0.3-5 x 10(28) amu/s, are much larger than the pre-Cassini estimates and also much larger than the measured ion loss rates (similar to 1-5 x 10(26) amu/s). If the largest heavy molecule escape rates are assumed, a significant fraction of the present atmosphere would have been lost to space in 4 Gyr. Because understanding the nature of the active escape processes is critical, a number of data sets were used to model the methane and nitrogen escape rates. The solar heating/cooling rate and the nitrogen density profile vs altitude were used in a fluid dynamic model to extract an average net upward flux below the exobase; the altitude dependence of the diffusion of methane through nitrogen was described below the exobase allowing for upward flow and escape; the coronal structure above the exobase was simulated by plasma and photon-induced hot particle production; and measurements of the emission from excited-dissociation products were used to estimate escape. In the latter two models, hot recoils from photochemistry or plasma-ion-induced heating lead to escape, whereas in the first two models heat conduction from below was assumed to enhance Jeans escape, a process referred to as slow hydrodynamic escape. These models are compared to each other and to recent simulations of Titan's exobase region. It is found that these simulations are inconsistent with the slow hydrodynamic escape model and that the composition of the magnetospheric plasma at Titan's orbit is inconsistent with the largest carbon loss rates suggested. C1 [Johnson, R. E.; Tucker, O. J.] Univ Virginia, Charlottesville, VA 22904 USA. [Johnson, R. E.; Tucker, O. J.] NYU, Dept Phys, New York, NY 10003 USA. [Michael, M.] Indian Inst Technol, Dept Civil Engn, Kanpur 208016, Uttar Pradesh, India. [Sittler, E. C.] GSFC, Greenbelt, MD USA. [Smith, H. T.] JHUAPL, Laurel, MD USA. [Young, D. T.; Waite, J. H.] SwRI, San Antonio, TX USA. RP Tucker, OJ (reprint author), Univ Virginia, Charlottesville, VA 22904 USA. EM rej@virginia.edu RI Smith, Howard/H-4662-2016 OI Smith, Howard/0000-0003-3537-3360 NR 88 TC 26 Z9 26 U1 0 U2 1 PU SPRINGER PI DORDRECHT PA PO BOX 17, 3300 AA DORDRECHT, NETHERLANDS BN 978-1-4020-9214-5 PY 2009 BP 373 EP 391 DI 10.1007/978-1-4020-9215-2_15 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BMN07 UT WOS:000272894300015 ER PT B AU Sittler, EC Hartle, RE Bertucci, C Coates, A Cravens, T Dandouras, I Shemansky, D AF Sittler, Edward C. Hartle, R. E. Bertucci, Cesar Coates, Andrew Cravens, Thomas Dandouras, Iannis Shemansky, Don BE Brown, RH Lebreton, JP Waite, JH TI Energy Deposition Processes in Titan's Upper Atmosphere and Its Induced Magnetosphere SO TITAN FROM CASSINI-HUYGENS LA English DT Article; Book Chapter ID FAR-ULTRAVIOLET SPECTROPHOTOMETRY; POLYCYCLIC AROMATIC-HYDROCARBONS; CASSINI PLASMA SPECTROMETER; FULLERENE RADICAL CATIONS; STRUCTURE INSTRUMENT HASI; MAGNETIC-FIELD; SATURNS MAGNETOSPHERE; E-RING; ELECTRICAL-CONDUCTIVITY; DUST MEASUREMENTS AB Most of Titan's atmospheric organic and nitrogen chemistry, aerosol formation, and atmospheric loss are driven from external energy sources such as Solar UV, Saturn's magnetosphere, solar wind and galactic cosmic rays. The Solar UV tends to dominate the energy input at lower altitudes similar to 1,200 km but which can extend down to similar to 400 km, while the plasma interaction from Saturn's magnetosphere, Saturn's magnetosheath or solar wind are more important at higher altitudes similar to 1,400 km, but the heavy ion plasma (O+) similar to 5 keV and energetic ions (H+) similar to 30 keV or higher from Saturn's magnetosphere can penetrate below 950 km. Cosmic rays with energies >1 GeV can penetrate much deeper into Titan's atmosphere with most of its energy deposited similar to 70 km altitude. Haze layers are observed in scattered solar photons starting at 510 km, but aerosols are broadly distributed and measured in extinction from 1,000 km downward, diffusively separated to 400 km. The induced magnetic field from Titan's interaction with the external plasma can be very complex and will tend to channel the flow of energy into Titan's upper atmosphere. Cassini observations combined with advanced hybrid simulations of the plasma interaction with Titan's upper atmosphere show significant changes in the character of the interaction with Saturn local time at Titan's orbit where the magnetosphere displays large and systematic changes with local time. The external solar wind can also drive sub-storms within the magnetosphere which can then modify the magnetospheric interaction with Titan. Another important parameter is solar zenith angle (SZA) with respect to the co-rotation direction of the magnetospheric flow which is referred to as the solar incidence-ram angle. Titan's interaction can contribute to atmospheric loss via pickup ion loss, scavenging of Titan's ionospheric plasma, loss of ionospheric plasma down its induced magnetotail via an ionospheric wind, and non-thermal loss of the atmosphere via heating and sputtering induced by the bombardment of magnetospheric keV ions and electrons. This energy input evidently drives the large positive and negative ions observed below similar to 1,100 km altitude with ion masses exceeding 10,000 Da. We refer to these ions as seed particles for the aerosols observed below 1,000 km altitude. These seed particles can be formed, for example, from the polymerization of acetylene (C2H2) and benzene (C6H6) molecules in Titan's upper atmosphere to form polycyclic aromatic hydrocarbons (PAH) and/or fullerenes (C-60). In the case of fullerenes, which are hollow spherical carbon shells, magnetospheric keV O+ ions can become trapped inside the fullerenes and eventually find themselves inside the aerosols as free oxygen. The aerosols are then expected to fall to Titan's surface as polymerized hydrocarbons with trapped free oxygen where unknown surface chemistry can take place. C1 [Sittler, Edward C.; Hartle, R. E.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Bertucci, Cesar] Inst Astron & Space Phys IAFE, Buenos Aires, DF, Argentina. [Coates, Andrew] UCL, Mullard Space Sci Lab, London WC1E 6BT, England. [Cravens, Thomas] Univ Kansas, Lawrence, KS 66045 USA. [Dandouras, Iannis] Ctr Etud Spatiale Rayonnements Lab, CNRS, Toulouse, France. [Shemansky, Don] Univ So Calif, Dept Aerosp & Mech Engn, Los Angeles, CA USA. RP Sittler, EC (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. EM Edward.C.Sittler@nasa.gov RI Coates, Andrew/C-2396-2008 OI Coates, Andrew/0000-0002-6185-3125 NR 213 TC 40 Z9 40 U1 0 U2 0 PU SPRINGER PI DORDRECHT PA PO BOX 17, 3300 AA DORDRECHT, NETHERLANDS BN 978-1-4020-9214-5 PY 2009 BP 393 EP 453 DI 10.1007/978-1-4020-9215-2_16 PG 61 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BMN07 UT WOS:000272894300016 ER PT B AU Hansen, CJ Waite, JH Bolton, SJ AF Hansen, C. J. Waite, J. H. Bolton, S. J. BE Brown, RH Lebreton, JP Waite, JH TI Titan in the Cassini-Huygens Extended Mission SO TITAN FROM CASSINI-HUYGENS LA English DT Article; Book Chapter ID ATMOSPHERIC TEMPERATURES; RADAR OBSERVATIONS; LANDING SITE; SURFACE; WINDS; SPECTROMETER; TOPOGRAPHY; IMAGES; ETHANE; OCEAN C1 [Hansen, C. J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Waite, J. H.; Bolton, S. J.] SW Res Inst, San Antonio, TX 78238 USA. RP Hansen, CJ (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM Candice.j.Hansen@jpl.nasa.gov NR 43 TC 1 Z9 1 U1 0 U2 0 PU SPRINGER PI DORDRECHT PA PO BOX 17, 3300 AA DORDRECHT, NETHERLANDS BN 978-1-4020-9214-5 PY 2009 BP 455 EP 477 DI 10.1007/978-1-4020-9215-2_17 PG 23 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BMN07 UT WOS:000272894300017 ER PT B AU Makeev, MA Lawson, JW Srivastava, D AF Makeev, Maxim A. Lawson, John W. Srivastava, Deepak GP TMS TI KINETICS OF FORMATION AND THERMAL AND MECHANICAL PROPERTIES OF CHAR OBTAINED BY ULTRA-HIGH TEMPERATURE PYROLYSIS OF POLYETHYLENE VIA MOLECULAR DYNAMICS SIMULATIONS SO TMS 2009 138TH ANNUAL MEETING & EXHIBITION - SUPPLEMENTAL PROCEEDINGS, VOL 2: MATERIALS CHARACTERIZATION, COMPUTATION AND MODELING LA English DT Proceedings Paper CT 138th TMS Annual Meeting and Exhibition CY FEB 15-19, 2009 CL San Francisco, CA DE pyrolytic char; atomistic simulations; elastic properties; thermal conductivity ID FLAMMABILITY PROPERTIES; CONDUCTIVITY; NANOCOMPOSITES; NETWORKS; FILMS AB We report results of a molecular dynamics simulation study of the high-temperature pyrolysis of polyethylene (PE) and the mechanical and thermal properties of the resultant carbonaceous char. The microstructure of pyrolyzed PE samples was monitored during the simulation. Mechanical properties of the resultant char were studied for char samples with varied microstructure (average coordination number and ring-size distributions) to establish structure-property relationships between mechanical (thermal) response properties and microstructure. We found that this relationship can be established based upon the random network theory of amorphous media, if additional topological constraints due to rings are taken into account. Thermal conductivity of pyrolytic char is investigated for samples with different microstructures for a wide range of temperatures. Similar to the mechanical response, the thermal response properties are correlated to microstructure. It is shown that the behavior of the thermal conductivity can be well described by Einstein's heat transfer theory, if microstructure effecs are taken into account. C1 [Makeev, Maxim A.; Lawson, John W.; Srivastava, Deepak] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Makeev, MA (reprint author), NASA, Ames Res Ctr, Mail Stop 229-1, Moffett Field, CA 94035 USA. NR 14 TC 0 Z9 0 U1 4 U2 10 PU MINERALS, METALS & MATERIALS SOC PI WARRENDALE PA 184 THORN HILL RD, WARRENDALE, PA 15086-7514 USA BN 978-0-87339-739-1 PY 2009 BP 79 EP 86 PG 8 WC Materials Science, Multidisciplinary; Metallurgy & Metallurgical Engineering; Materials Science, Characterization & Testing; Mineralogy SC Materials Science; Metallurgy & Metallurgical Engineering; Mineralogy GA BJC16 UT WOS:000264674700011 ER PT S AU Rowe, JF Matthews, JM Seager, S Sasselov, D Kuschnig, R Guenther, DB Moffat, AFJ Rucinski, SM Walker, GAH Weiss, WW AF Rowe, Jason F. Matthews, Jaymie M. Seager, Sara Sasselov, Dimitar Kuschnig, Rainer Guenther, David B. Moffat, Anthony F. J. Rucinski, Slavek M. Walker, Gordon A. H. Weiss, Werner W. BE Pont, F Sasselov, D Holman, M TI Towards the Albedo of an Exoplanet: MOST Satellite Observations of Bright Transiting Exoplanetary Systems SO TRANSITING PLANETS, PROCEEDINGS SE IAU Symposium Proceedings Series LA English DT Proceedings Paper CT 253th Symposium of the International-Astronomical-Union CY MAY 19-23, 2008 CL Cambridge, MA SP Int Astron Union ID HD 209458B; ATMOSPHERES; PHOTOMETRY; CLOUDS; SPACE AB The Canadian MOST satellite is a unique platform for observations of bright transiting exoplanetary systems. Providing nearly continuous photometric observations for lip to 4 weeks, MOST can produce important observational data, to hell) us learn about the properties of exosolar planets. We review our current, observations of HD 209458 and HD 189733 with implications for the albedo and our progress towards detecting reflected light from an exoplanet. C1 [Rowe, Jason F.; Matthews, Jaymie M.; Seager, Sara; Sasselov, Dimitar; Kuschnig, Rainer; Guenther, David B.; Moffat, Anthony F. J.; Rucinski, Slavek M.; Walker, Gordon A. H.; Weiss, Werner W.] NASA, Moffett Field, CA 94035 USA. RP Rowe, JF (reprint author), NASA, Ames Res Pk,MS-244-30, Moffett Field, CA 94035 USA. EM jasonfrowe@gmail.com; matthews@astro.ubc.ca; seager@mit.edu; dsasselov@cfa.harvard.edu; dsasselov@cfa.harvard.edu NR 11 TC 0 Z9 0 U1 0 U2 0 PU CAMBRIDGE UNIV PRESS PI CAMBRIDGE PA THE PITT BUILDING, TRUMPINGTON ST, CAMBRIDGE CB2 1RP, CAMBS, ENGLAND SN 1743-9213 BN 978-0-521-88984-1 J9 IAU SYMP P SERIES JI IAU Symposium Proc. Series PY 2009 VL 4 IS 253 BP 121 EP 127 DI 10.1017/S1743921308026318 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BJD37 UT WOS:000264979500014 ER PT S AU Deming, D AF Deming, Drake BE Pont, F Sasselov, D Holman, M TI Emergent Exoplanet Flux: Review of the Spitzer Results SO TRANSITING PLANETS, PROCEEDINGS SE IAU Symposium Proceedings Series LA English DT Proceedings Paper CT 253th Symposium of the International-Astronomical-Union CY MAY 19-23, 2008 CL Cambridge, MA SP Int Astron Union ID PLANET HD 189733B; TRANSITING EXTRASOLAR PLANET; HOT JUPITERS; SPACE-TELESCOPE; ATMOSPHERIC CIRCULATION; THERMAL EMISSION; INFRARED RADIUS; 209458B; SPECTRUM; WATER AB Observations using the Spitzer Space Telescope provided the first; detections of photons from extrasolar planets. Spitzer observations are allowing us to infer the temperature structure, composition, and dynamics of exoplanet atmospheres. The Spitzer studies extend from many hot Jupiters to the hot Neptune orbiting GJ 436. Here I review the current status of Spitzer secondary eclipse observations, and summarize the results from the viewpoint, of what is robust, what needs more work, and what the observations are telling us about the physical nature of exoplanet atmospheres. C1 NASA, Goddard Space Flight Ctr, Planetary Syst Lab, Greenbelt, MD 20771 USA. RP Deming, D (reprint author), NASA, Goddard Space Flight Ctr, Planetary Syst Lab, Code 693, Greenbelt, MD 20771 USA. EM ddeming@pop600.gsfc.nasa.gov NR 43 TC 0 Z9 0 U1 0 U2 0 PU CAMBRIDGE UNIV PRESS PI CAMBRIDGE PA THE PITT BUILDING, TRUMPINGTON ST, CAMBRIDGE CB2 1RP, CAMBS, ENGLAND SN 1743-9213 BN 978-0-521-88984-1 J9 IAU SYMP P SERIES JI IAU Symposium Proc. Series PY 2009 VL 4 IS 253 BP 197 EP 207 DI 10.1017/S1743921308026410 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BJD37 UT WOS:000264979500023 ER PT S AU Borucki, W Koch, D Batalha, N Caldwell, D Christensen-Dalsgaard, J Cochran, WD Dunham, E Gautier, TN Geary, J Gilliland, R Jenkins, J Kjeldsen, H Lissauer, JJ Rowe, J AF Borucki, William Koch, David Batalha, Natalie Caldwell, Douglas Christensen-Dalsgaard, Jorgen Cochran, William D. Dunham, Edward Gautier, Thomas N. Geary, John Gilliland, Ronald Jenkins, Jon Kjeldsen, Hans Lissauer, Jack J. Rowe, Jason BE Pont, F Sasselov, D Holman, M TI KEPLER: Search for Earth-Size Planets in the Habitable Zone SO TRANSITING PLANETS, PROCEEDINGS SE IAU Symposium Proceedings Series LA English DT Proceedings Paper CT 253th Symposium of the International-Astronomical-Union CY MAY 19-23, 2008 CL Cambridge, MA SP Int Astron Union ID PHOTOMETRIC-METHOD; COMPANION; SYSTEMS; STARS AB The Kepler Mission is a space-based mission whose primary goal is to determine the frequency of Earth-size and larger planets in the habitable zone of solar-like stars. The mission will monitor more than 100,000 stars for patterns of transits with a differential photometric precision of 20 ppm at V = 12 for a 6.5 hour transit. It will also provide asteroseismic results on several thousand dwarf stars. It is specifically designed to continuously observe a single field of view of greater than 100 square degrees for 3.5 or more years. This paper provides a short overview of the mission, a brief history of the mission development, expected results, new investigations by the recently chosen Participating Scientists, and the plans for the Guest Observer and Astrophysical Data, Programs. C1 [Borucki, William; Koch, David; Lissauer, Jack J.; Rowe, Jason] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Borucki, W (reprint author), NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. EM henry.w.daniels-l@nasa.gov; dkoch@mail.arc.nasa.gov; Thomas.N.Gautier@jpl.nasa.gov; gillil@stsci.edu; hans@phys.au.dk; jlissauer@mail.arc.nasa.gov; jasonfrowe@gmail.com RI Caldwell, Douglas/L-7911-2014 OI Caldwell, Douglas/0000-0003-1963-9616 NR 21 TC 5 Z9 5 U1 1 U2 1 PU CAMBRIDGE UNIV PRESS PI CAMBRIDGE PA THE PITT BUILDING, TRUMPINGTON ST, CAMBRIDGE CB2 1RP, CAMBS, ENGLAND SN 1743-9213 BN 978-0-521-88984-1 J9 IAU SYMP P SERIES JI IAU Symposium Proc. Series PY 2009 VL 4 IS 253 BP 289 EP 299 DI 10.1017/S1743921308026513 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BJD37 UT WOS:000264979500033 ER PT S AU Iro, N Deming, D AF Iro, Nicolas Deming, Drake BE Pont, F Sasselov, D Holman, M TI A time-dependent radiative model for the atmosphere of the eccentric transiting planets SO TRANSITING PLANETS, PROCEEDINGS SE IAU Symposium Proceedings Series LA English DT Proceedings Paper CT 253th Symposium of the International-Astronomical-Union CY MAY 19-23, 2008 CL Cambridge, MA SP Int Astron Union AB We present a time-dependent radiative model for the atmosphere of the transiting planets that takes into account the eccentricity of their orbit. We investigate the temporal temperature and flux variations due to the planet-star distance variability. We will also discuss observational aspects with Spitzer measurements. C1 [Iro, Nicolas; Deming, Drake] NASA, GSFC Planetary Syst Lab Code 693 0, Greenbelt, MD 20770 USA. RP Iro, N (reprint author), NASA, GSFC Planetary Syst Lab Code 693 0, Greenbelt, MD 20770 USA. EM nicolas.iro@nasa.gov; leo.d.deming@nasa.gov NR 7 TC 0 Z9 0 U1 0 U2 0 PU CAMBRIDGE UNIV PRESS PI CAMBRIDGE PA THE PITT BUILDING, TRUMPINGTON ST, CAMBRIDGE CB2 1RP, CAMBS, ENGLAND SN 1743-9213 BN 978-0-521-88984-1 J9 IAU SYMP P SERIES JI IAU Symposium Proc. Series PY 2009 VL 4 IS 253 BP 516 EP 519 DI 10.1017/S1743921308027099 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BJD37 UT WOS:000264979500090 ER PT S AU O'Donovan, FT Charbonneau, D Harrington, J Seager, S Deming, D Knutson, HA AF O'Donovan, Francis T. Charbonneau, David Harrington, Joseph Seager, Sara Deming, Drake Knutson, Heather A. BE Pont, F Sasselov, D Holman, M TI Detection of Planetary Emission from TrES-2 using Spitzer/IRAC SO TRANSITING PLANETS, PROCEEDINGS SE IAU Symposium Proceedings Series LA English DT Proceedings Paper CT 253th Symposium of the International-Astronomical-Union CY MAY 19-23, 2008 CL Cambridge, MA SP Int Astron Union ID TRANSITS; PROJECT AB We present here results from observations of TrES-2 made using the Infrared Array Camera on the Spitzer Space Telescope. We monitored this transiting system during two secondary eclipses, when the planetary emission is blocked by the star. The resulting decrease in flux is 0.135 +/- 0.036%, 0.245 +/- 0.027%, 0.162 +/- 0.064%, and 0.295 +/- 0.066%, at 3.6-mu m, 4.5-mu m, 5.8-mu m, and 8.0-mu m, respectively. We find evidence for a temperature inversion in the atmosphere of TrES-2. which is predicted by Fortney and collaborators based on the proposed importance of TiO and VO opacities for this highly irradiated gas giant. We also find the time of the center of the eclipse to be consistent with predictions from transit timing observations of TrES-2. This implies that TrES-2 most likely has a circular orbit, and thus does not obtain additional thermal energy from tidal dissipation of a non-zero orbital eccentricity, a proposed explanation of the large planetary radius. C1 [O'Donovan, Francis T.; Deming, Drake] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP O'Donovan, FT (reprint author), NASA, Goddard Space Flight Ctr, 8800 Greenbelt Rd, Greenbelt, MD 20771 USA. EM francis.odonovan@nasa.gov; dcharbonneau@cfa.harvard.edu; jh@physics.ucf.edu; seager@mit.edu; leo.d.deming@nasa.gov; hknutson@cfa.harvard.edu OI Charbonneau, David/0000-0002-9003-484X NR 8 TC 0 Z9 0 U1 0 U2 0 PU CAMBRIDGE UNIV PRESS PI CAMBRIDGE PA THE PITT BUILDING, TRUMPINGTON ST, CAMBRIDGE CB2 1RP, CAMBS, ENGLAND SN 1743-9213 BN 978-0-521-88984-1 J9 IAU SYMP P SERIES JI IAU Symposium Proc. Series PY 2009 VL 4 IS 253 BP 536 EP 539 DI 10.1017/S1743921308027142 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BJD37 UT WOS:000264979500095 ER PT J AU Ducluzeau, AL van Lis, R Duval, S Schoepp-Cothenet, B Russell, MJ Nitschke, W AF Ducluzeau, Anne-Lise van Lis, Robert Duval, Simon Schoepp-Cothenet, Barbara Russell, Michael J. Nitschke, Wolfgang TI Was nitric oxide the first deep electron sink? SO TRENDS IN BIOCHEMICAL SCIENCES LA English DT Review ID COPPER OXYGEN REDUCTASES; CYTOCHROME-C-OXIDASE; ACTIVE-SITE RESIDUE; NITROGEN-FIXATION; CBB(3) OXIDASES; OXIDATION-STATE; EARLY EVOLUTION; EARLY EARTH; ATMOSPHERE; REDOX AB Evolutionary histories of enzymes involved in chemiosmotic energy conversion indicate that a strongly oxidizing substrate was available to the last universal common ancestor before the divergence of Bacteria and Archaea. According to palaeogeochemical evidence, 02 was not present beyond trace amounts on the early Earth. Based on recent phylogenetic, enzymatic and geochemical results, we propose that, in the earliest Archaean, nitric oxide (NO) and its derivatives nitrate and nitrite served as strongly oxidizing substrates driving the evolution of a bioenergetic pathway related to modern dissimilatory denitrification. Aerobic respiration emerged later from within this ancestral pathway via adaptation of the enzyme NO reductase to its new substrate, dioxygen. C1 [Ducluzeau, Anne-Lise; van Lis, Robert; Duval, Simon; Schoepp-Cothenet, Barbara; Nitschke, Wolfgang] CNRS, Lab Bioenerget & Ingn Prot, UPR9036, IFR77, F-13402 Marseille 20, France. [Russell, Michael J.] CALTECH, Jet Prop Lab, Sect 3220, Pasadena, CA 91109 USA. RP Nitschke, W (reprint author), CNRS, Lab Bioenerget & Ingn Prot, UPR9036, IFR77, 31 Chemin Joseph Aiguier, F-13402 Marseille 20, France. EM nitschke@ibsm.cnrs-mrs.fr OI Nitschke, Wolfgang/0000-0003-2084-3032 FU French Agence Nationale pour la Recherche [ANR-06-BLAN-0384]; National Aeronautics and Space Administration FX We thank Christaphe Leger (Marseille) and Chris Boxe (Jet Propulsion Laboratory) for stimulating discussions, Our work was financially supported by the French Agence Nationale pour la Recherche (ANR-06-BLAN-0384 and ERRMoE; www.agence-nationale-recherche.fr). M.J.R.'s research described here was carried out at the Jet Propulsion Laboratory, California Institute of Technology (www.jpl.nasa.gov) under a contract with the National Aeronautics and Space Administration (www.nasa.gov). NR 49 TC 68 Z9 69 U1 3 U2 25 PU ELSEVIER SCIENCE LONDON PI LONDON PA 84 THEOBALDS RD, LONDON WC1X 8RR, ENGLAND SN 0968-0004 J9 TRENDS BIOCHEM SCI JI Trends Biochem.Sci. PD JAN PY 2009 VL 34 IS 1 BP 9 EP 15 DI 10.1016/j.tibs.2008.10.005 PG 7 WC Biochemistry & Molecular Biology SC Biochemistry & Molecular Biology GA 402HY UT WOS:000263006000006 PM 19008107 ER PT J AU Dellacorte, C AF Dellacorte, Christopher TI History's ultimate lube job SO TRIBOLOGY & LUBRICATION TECHNOLOGY LA English DT Article C1 NASA, Glenn Res Ctr, Cleveland, OH USA. RP Dellacorte, C (reprint author), NASA, Glenn Res Ctr, Cleveland, OH USA. EM christopher.dellocorte@nasa.gov NR 0 TC 0 Z9 0 U1 0 U2 0 PU SOC TRIBOLOGISTS & LUBRICATION ENGINEERS PI PARK RIDGE PA 840 BUSSE HIGHWAY, PARK RIDGE, IL 60068 USA SN 1545-858X J9 TRIBOL LUBR TECHNOL JI Tribol. Lubr. Technol. PD JAN PY 2009 VL 65 IS 1 BP 26 EP 27 PG 2 WC Engineering, Mechanical SC Engineering GA 397RL UT WOS:000262679700008 ER PT J AU Stanford, MK AF Stanford, Malcolm K. TI Dimensional Stability, Microstructure, and Cohesion Strength of Composite Solid Lubricant Coatings after Heat Treatment SO TRIBOLOGY TRANSACTIONS LA English DT Article DE Plasma Spray Coatings; Lubrication; Cohesion; Metallography; Oxidation ID TEMPERATURE; PS304 AB PS304 is a plasma spray deposited coating composed of Ni-Cr, Cr(2)O(3), Ag, and BaF(2)-CaF(2) that has been developed for reduction of friction and wear at high temperatures. Physical properties of the coating after varying heat treatments and using varying weight percentages of chromium in the Ni-Cr constituent have been investigated. Dimensional stability was reduced with increasing heat treatment temperature and the coating growth rate decreased with time. The dimensional stability was also reduced as the Cr content in the Ni-Cr constituent increased from 10 to 30 wt%. Coating growth was due to oxidation of the Ni-Cr constituent. The optimum cohesion strength for PS304 was essentially the same after heat treatment at 650 or 725 degrees C for 100 h. Further investigation indicated that heat treatment at 725 degrees C for 100 h increases the dimensional stability in a high temperature service environment. C1 NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. RP Stanford, MK (reprint author), NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. NR 14 TC 1 Z9 1 U1 1 U2 2 PU TAYLOR & FRANCIS INC PI PHILADELPHIA PA 325 CHESTNUT ST, SUITE 800, PHILADELPHIA, PA 19106 USA SN 1040-2004 J9 TRIBOL T JI Tribol. Trans. PY 2009 VL 52 IS 2 BP 269 EP 276 DI 10.1080/10402000802527781 PG 8 WC Engineering, Mechanical SC Engineering GA 424GR UT WOS:000264554600004 ER PT J AU Morales, W Handschuh, RF Krantz, TL AF Morales, Wilfredo Handschuh, Robert F. Krantz, Timothy L. TI Feasibility Study of Vapor-Mist Phase Reaction Lubrication using a Thioether Liquid SO TRIBOLOGY TRANSACTIONS LA English DT Article DE Gears; Vapor Phase Lubrication ID IRON AB Aerospace drive systems are required to survive a loss-of-lubrication test for qualification. In many cases emergency lubrication systems need to be designed and utilized to permit the drive system to pass this difficult requirement. The weight of emergency systems can adversely affect the mission capabilities of the aircraft. The possibility to reduce the emergency system weight using vapor-mist phase lubrication (VMPL) technology has been considered by NASA and the Army Research Laboratory (ARL). Phosphate esters have been the lubricant of choice in most VMPL studies primarily because they do provide adequate lubrication for short periods of time. However, during the lubrication process, the phosphate esters react continuously with the surface iron in gears and bearings, resulting in excessive wear. To minimize this problem an alternative non-phosphate liquid, a thioether, was used to mist phase lubricate a spur gearbox rig operating at 10,000 rpm under highly loaded conditions. After 21 million shaft revolutions of operation the gears exhibited only minor wear. C1 [Morales, Wilfredo] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. [Handschuh, Robert F.; Krantz, Timothy L.] US Army Res Lab, Glenn Res Ctr, Cleveland, OH 44135 USA. RP Morales, W (reprint author), NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. NR 11 TC 1 Z9 2 U1 0 U2 3 PU TAYLOR & FRANCIS INC PI PHILADELPHIA PA 325 CHESTNUT ST, SUITE 800, PHILADELPHIA, PA 19106 USA SN 1040-2004 J9 TRIBOL T JI Tribol. Trans. PY 2009 VL 52 IS 3 BP 370 EP 375 DI 10.1080/10402000802563448 PG 6 WC Engineering, Mechanical SC Engineering GA 424GS UT WOS:000264554700004 ER PT J AU Oswald, FB Zaretsky, EV Poplawski, JV AF Oswald, Fred B. Zaretsky, Erwin V. Poplawski, Joseph V. TI Interference-Fit Life Factors for Roller Bearings SO TRIBOLOGY TRANSACTIONS LA English DT Article DE Interference Fit; Cylindrical Roller Bearings; Rolling Bearings; Fatigue Analysis; Contacts; Life Prediction Methods; Maintenance; Rolling Bearings; Rolling-Contact Fatigue; Wear; Stress Analysis; Contacts ID PREDICTION; PROFILE AB The effect of hoop stresses in reducing cylindrical roller bearing fatigue life was determined for various classes of inner-ring interference fit. Calculations were performed for up to seven fit classes for each of the 10 bearing sizes. The hoop stresses were superimposed on the Hertzian principal stresses created by the applied radial load to calculate roller bearing fatigue life. A method was developed through a series of equations to calculate the life reduction for cylindrical roller bearings. All calculated lives are for zero initial internal clearance. Any reduction in bearing clearance due to interference fit would be compensated by increasing the initial (unmounted) clearance. The results are presented as tables and charts of life factors for bearings with light, moderate, and heavy loads and interference fits ranging from extremely light to extremely heavy for bearing accuracy class RBEC-5 (ISO class 5). Interference fits on the inner ring of a cylindrical roller bearing can significantly reduce bearing fatigue life. In general, life factors are smaller (lower life) for bearings running under a light load where the unfactored life is the highest. The various bearing series within a particular bore size had almost identical interference-fit life factors for a particular fit. The tightest fit at the high end of the tolerance band produces a life factor of approximately 0.40 for an inner-race maximum Hertz stress of 1200 MPa (175 ksi) and a life factor of 0.60 for an inner-race maximum Hertz stress of 2200 MPa (320 ksi). Interference fits also impact the maximum Hertz stress-life relation. C1 [Oswald, Fred B.; Zaretsky, Erwin V.] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. [Poplawski, Joseph V.] JV Poplawski & Associates, Bethlehem, PA 18018 USA. RP Oswald, FB (reprint author), NASA, Glenn Res Ctr, 21000 Brookpk Rd, Cleveland, OH 44135 USA. NR 19 TC 6 Z9 8 U1 0 U2 4 PU TAYLOR & FRANCIS INC PI PHILADELPHIA PA 325 CHESTNUT ST, SUITE 800, PHILADELPHIA, PA 19106 USA SN 1040-2004 J9 TRIBOL T JI Tribol. Trans. PY 2009 VL 52 IS 4 BP 415 EP 426 AR PII 910296043 DI 10.1080/10402000802687890 PG 12 WC Engineering, Mechanical SC Engineering GA 434VK UT WOS:000265302000001 ER PT J AU Miller, BA Howard, SA AF Miller, Brad A. Howard, Samuel A. TI Identifying Bearing Rotor-Dynamic Coefficients Using an Extended Kalman Filter SO TRIBOLOGY TRANSACTIONS LA English DT Article DE Hydrodynamic Bearings; Journal Bearings; Dynamic Modeling ID 2 JOURNAL BEARINGS; SUPPORT PARAMETERS; FIELD METHODS; IDENTIFICATION; RESPONSES AB An extended Kalman filter is developed to estimate the linearized direct and indirect stiffness and damping force coefficients for bearings in rotor-dynamic applications from noisy measurements of the shaft displacement in response to imbalance and impact excitation. The bearing properties are modeled as stochastic random variables using a Gauss-Markov model. Noise terms are introduced into the system model to account for all of the estimation error, including modeling errors and uncertainties and the propagation of measurement errors into the parameter estimates. The system model contains two user-defined parameters that can be tuned to improve the filter's performance; these parameters correspond to the covariance of the system and measurement noise variables. The filter is also strongly influenced by the initial values of the states and the error covariance matrix. The filter is demonstrated using numerically simulated data for a rotor-bearing system with two identical bearings, which reduces the number of unknown linear dynamic coefficients to eight. The filter estimates the direct damping coefficients and all four stiffness coefficients correlated well with actual values, whereas the estimates the cross-coupled damping coefficients were the least accurate. C1 [Miller, Brad A.] Harding Univ, Dept Engn & Phys, Searcy, AR 72149 USA. [Howard, Samuel A.] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. RP Miller, BA (reprint author), Harding Univ, Dept Engn & Phys, 915 E Market Ave, Searcy, AR 72149 USA. FU NASA [NNC06GA20G] FX The material is based upon work supported by NASA under award No. NNC06GA20G. NR 19 TC 2 Z9 2 U1 0 U2 1 PU TAYLOR & FRANCIS INC PI PHILADELPHIA PA 325 CHESTNUT ST, SUITE 800, PHILADELPHIA, PA 19106 USA SN 1040-2004 J9 TRIBOL T JI Tribol. Trans. PY 2009 VL 52 IS 5 BP 671 EP 679 AR PII 913558721 DI 10.1080/10402000902913295 PG 9 WC Engineering, Mechanical SC Engineering GA 481RZ UT WOS:000268830700003 ER PT S AU Goldstein, ML AF Goldstein, Melvyn L. BE Hasan, SS Gangadhara, RT Krishan, V TI Observations and Modeling of Turbulence in the Solar Wind SO TURBULENCE, DYNAMOS, ACCRETION DISKS, PULSARS AND COLLECTIVE PLASMA PROCESSES SE Astrophysics and Space Science Proceedings LA English DT Proceedings Paper CT 1st Kodai-Trieste Workshop on Plasma Astrophysics CY AUG 27-SEP 07, 2007 CL Kodaikanal, INDIA SP Indian Inst Astrophys, Kodaikanal Observatory, Abdus Salam Int Ctr Theoret Phys DE Magnetohydrodynamics-solar wind; Turbulence-simulations ID INTERPLANETARY MAGNETIC-FIELD; FLUX-CORRECTED TRANSPORT; MAGNETOHYDRODYNAMIC FLUCTUATIONS; HELIOS OBSERVATIONS; VELOCITY SHEAR; ALFVEN WAVES; EVOLUTION; SIMULATION; ANISOTROPY; LATITUDES AB Alfvenic fluctuations are a ubiquitous component of the solar wind. Evidence from many spacecrafts indicate that the fluctuations are convected out of the solar corona with relatively flat power spectra and constitute a source of free energy for a turbulent cascade of magnetic and kinetic energy to high wave numbers. Observations and simulations support the conclusion that the cascade evolves most, rapidly in the vicinity of velocity shears and current sheets. Numerical solutions of the magnetohydrodynamic equations have elucidated the role of expansion on the evolution of the turbulence. Such studies are clarifying not only how a turbulent cascade develops, but, also the nature of the symmetries of the turbulence. C1 NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Goldstein, ML (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. EM melvyn.l.goldstein@nasa.gov RI Goldstein, Melvyn/B-1724-2008 NR 44 TC 1 Z9 1 U1 0 U2 1 PU SPRINGER PI DORDRECHT PA PO BOX 17, 3300 AA DORDRECHT, NETHERLANDS SN 1570-6591 BN 978-1-4020-8867-4 J9 ASTROPHYSICS SPACE PY 2009 BP 21 EP 33 PG 13 WC Astronomy & Astrophysics; Physics, Fluids & Plasmas SC Astronomy & Astrophysics; Physics GA BIY36 UT WOS:000263688100002 ER PT S AU Chiuderi, C Velli, M AF Chiuderi, C. Velli, M. BE Vlahos, L Cargill, P TI Solar MHD: An Introduction SO TURBULENCE IN SPACE PLASMAS SE Lecture Notes in Physics LA English DT Article; Book Chapter ID ALFVEN WAVES; MAGNETOHYDRODYNAMIC TURBULENCE; CORONA; ENERGY; FIELDS; LOOPS C1 [Chiuderi, C.] Univ Florence, Dipartimento Astron, I-50125 Florence, Italy. [Velli, M.] CALTECH, Jet Prop Lab, Pasadena, CA USA. RP Chiuderi, C (reprint author), Univ Florence, Dipartimento Astron, Largo Enrico Fermi 5, I-50125 Florence, Italy. EM chiuderi@arcetri.astro.it; velli@arcetri.astro.it NR 38 TC 0 Z9 0 U1 1 U2 2 PU SPRINGER-VERLAG BERLIN PI BERLIN PA HEIDELBERGER PLATZ 3, D-14197 BERLIN, GERMANY SN 0075-8450 BN 978-3-642-00209-0 J9 LECT NOTES PHYS PY 2009 VL 778 BP 45 EP 69 DI 10.1007/978-3-642-00210-6_2 D2 10.1007/978-3-642-00210-6 PG 25 WC Astronomy & Astrophysics; Physics, Fluids & Plasmas SC Astronomy & Astrophysics; Physics GA BJZ20 UT WOS:000267515600003 ER PT S AU Velli, M AF Velli, M. BE Vlahos, L Cargill, P TI Physical Processes in the Solar Wind SO TURBULENCE IN SPACE PLASMAS SE Lecture Notes in Physics LA English DT Article; Book Chapter ID INTERPLANETARY ALFVENIC FLUCTUATIONS; MHD TURBULENCE; MAGNETOHYDRODYNAMIC TURBULENCE; HYDROMAGNETIC TURBULENCE; STELLAR WINDS; CORONAL HOLE; WAVES; ATMOSPHERE; EVOLUTION; DYNAMICS C1 [Velli, M.] Univ Florence, Dipartimento Astron, I-50125 Florence, Italy. [Velli, M.] CALTECH, Jet Prop Lab, Pasadena, CA USA. RP Velli, M (reprint author), Univ Florence, Dipartimento Astron, Largo Enrico Fermi 5, I-50125 Florence, Italy. EM velli@arcetri.astro.it NR 51 TC 1 Z9 1 U1 1 U2 1 PU SPRINGER-VERLAG BERLIN PI BERLIN PA HEIDELBERGER PLATZ 3, D-14197 BERLIN, GERMANY SN 0075-8450 BN 978-3-642-00209-0 J9 LECT NOTES PHYS PY 2009 VL 778 BP 247 EP 268 DI 10.1007/978-3-642-00210-6_7 D2 10.1007/978-3-642-00210-6 PG 22 WC Astronomy & Astrophysics; Physics, Fluids & Plasmas SC Astronomy & Astrophysics; Physics GA BJZ20 UT WOS:000267515600008 ER PT B AU Kurylo, MJ AF Kurylo, Michael J. BE Zerefos, C Contopoulos, G Skalkeas, G TI The Role of Airborne Science in the Study of Polar Ozone SO TWENTY YEARS OF OZONE DECLINE LA English DT Proceedings Paper CT Symposium for the 20th Anniversary of the Montreal Protocol 2007 CY SEP, 2007 CL Athens, GREECE SP United Nat Environm Programme, Int Ozone Commiss, Acad Athens, Mariolopoulos-Kanaginis Fdn DE Airborne science; integrated observations; ozone depletion; ozone hole; Polar Ozone ID ANTARCTICA AB This chapter will provide a brief historical perspective of the Antarctic ozone hole and the role that 1986-1987 ground-based and aircraft studies played in linking its formation to reactions involving chlorine and bromine radicals resulting from the degradation of halocarbon source gases (emitted in large part from human activities). The results from later aircraft campaigns focused oil understanding ozone production and loss within the Arctic stratosphere will also be highlighted. These results affirm the continuing need in ozone research for the integration of synoptic scale satellite measurements with ground-based, balloon-borne, and aircraft measurements having a unique temporal and spatial resolution. C1 NASA Headquarters, Sci Miss Directorate, Washington, DC USA. RP Kurylo, MJ (reprint author), NASA Headquarters, Sci Miss Directorate, Washington, DC USA. EM Michael.J.Kurylo@nasa.gov RI Kurylo, Michael/H-2201-2012 NR 2 TC 0 Z9 0 U1 0 U2 0 PU SPRINGER PI NEW YORK PA 233 SPRING STREET, NEW YORK, NY 10013, UNITED STATES BN 978-90-481-2468-8 PY 2009 BP 173 EP 182 DI 10.1007/978-90-481-2469-5_12 PG 10 WC Geochemistry & Geophysics; Environmental Sciences; Meteorology & Atmospheric Sciences SC Geochemistry & Geophysics; Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences GA BKP72 UT WOS:000268885100012 ER PT B AU Bhartia, PK AF Bhartia, Pawan K. BE Zerefos, C Contopoulos, G Skalkeas, G TI Role of Satellite Measurements in the Discovery of Stratospheric Ozone Depletion SO TWENTY YEARS OF OZONE DECLINE LA English DT Proceedings Paper CT Symposium for the 20th Anniversary of the Montreal Protocol 2007 CY SEP, 2007 CL Athens, GREECE SP United Nat Environm Programme, Int Ozone Commiss, Acad Athens, Mariolopoulos-Kanaginis Fdn DE Ozone hole; satellite algorithm; TOMS; total ozone; UVB AB This chapter discusses the role satellite total ozone measuring instruments have played in the study of stratospheric ozone depletion. By the early 1980s total ozone measured from two NASA satellites had produced a record that spanned more than a decade, with quality comparable with best ground-based stations. It was therefore a puzzle to many why NASA did not report the discovery of the Antarctic ozone depletion until late 1985. This was initially described as a computer error and continues to be described that way in both scientific and popular media. This simplistic labelling has unfortunately served to hide deeper issues about the ability of satellite instruments in making new scientific discoveries as the nature of the satellite retrieval problems make them critically dependent on the availability of prior information. Lack of such prior information and the unavailability of "ground-truth" data were key contributing factors that caused the delay in reporting the discovery of the Antarctic ozone hole, though it was clearly seen in the data by the summer of 1984. The strength of the satellite instruments is their capability to expand the limited view provided by ground-based and aircraft instruments into a global view. This view played a crucial role in making the public and policy makers aware of the seriousness of the ozone depletion problem that led to the phase-out of the ozone-destroying chemicals. This case is even stronger for the surface UV radiation where large spatial and temporal variability due to clouds and aerosols make it very difficult to see patterns in the data without the perspective that only satellites can provide. C1 NASA, Goddard Space Flight Ctr, Atmospheres Lab, Greenbelt, MD 20771 USA. RP Bhartia, PK (reprint author), NASA, Goddard Space Flight Ctr, Atmospheres Lab, Greenbelt, MD 20771 USA. EM Pawiin.Bhartia@nast.gov RI Bhartia, Pawan/A-4209-2016 OI Bhartia, Pawan/0000-0001-8307-9137 NR 13 TC 0 Z9 0 U1 0 U2 1 PU SPRINGER PI NEW YORK PA 233 SPRING STREET, NEW YORK, NY 10013, UNITED STATES BN 978-90-481-2468-8 PY 2009 BP 183 EP 189 DI 10.1007/978-90-481-2469-5_13 PG 7 WC Geochemistry & Geophysics; Environmental Sciences; Meteorology & Atmospheric Sciences SC Geochemistry & Geophysics; Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences GA BKP72 UT WOS:000268885100013 ER PT B AU Newman, PA Nash, ER Douglass, AR Nielsen, JE Stolarski, RS AF Newman, Paul A. Nash, Eric R. Douglass, Anne R. Nielsen, J. Eric Stolarski, Richard S. BE Zerefos, C Contopoulos, G Skalkeas, G TI Estimating When the Antarctic Ozone Hole will Recover SO TWENTY YEARS OF OZONE DECLINE LA English DT Proceedings Paper CT Symposium for the 20th Anniversary of the Montreal Protocol 2007 CY SEP, 2007 CL Athens, GREECE SP United Nat Environm Programme, Int Ozone Commiss, Acad Athens, Mariolopoulos Kanaginis Fdn DE Antarctic; ozone depletion; ozone hole; recovery; stratosphere ID CHLORINE; LOSSES AB The Antarctic ozone hole develops during the Austral winter and reaches its deepest levels by early spring (late September to early October). The severity of the hole has been assessed from satellites by calculating the average aerial coverage of depletion during the September-October period. Profile information shows that ozone is completely destroyed in the 14-21 km layer by early October. This ozone is mainly destroyed by halogen (chlorine and bromine) catalytic cycles, and these losses are modulated by temperature variations. Because atmospheric halogen levels are responding to international agreements that limit or phase out production, the amount of halogens in the stratosphere should considerably decrease over the next few decades. Using projections of halogen levels combined with age-of-air estimates, we find that the ozone hole is recovering at an extremely slow rate and that large ozone holes will regularly recur over the next 2 decades. We estimate that the ozone hole will begin to show first signs of area decrease in about 2023, and the hole will fully recover to pre-1980 levels in approximately 2070. Estimates of the ozone hole's recovery from models reveal important uncertainties in recovery as a result of climate change. C1 [Newman, Paul A.; Douglass, Anne R.; Stolarski, Richard S.] NASA, Goddard Space Flight Ctr, Atmospher Chem & Dynam Branch, Code 613-3, Greenbelt, MD 20771 USA. [Nash, Eric R.; Nielsen, J. Eric] Sci Syst & Appl Inc, Lanham, MD 20706 USA. RP Newman, PA (reprint author), NASA, Goddard Space Flight Ctr, Atmospher Chem & Dynam Branch, Code 613-3, Greenbelt, MD 20771 USA. EM Paul.A.Newman@nasa.gov RI Newman, Paul/D-6208-2012; Douglass, Anne/D-4655-2012; Stolarski, Richard/B-8499-2013 OI Newman, Paul/0000-0003-1139-2508; Stolarski, Richard/0000-0001-8722-4012 FU NASA FX This analysis work was mainly supported under a NASA grant for the Atmospheric Chemistry and Analysis Program (ACMAP), while the GEOS CCM modeling work was supported under a grant from the NASA Modeling, Analysis and Prediction (MAP) Program NR 24 TC 0 Z9 1 U1 1 U2 14 PU SPRINGER PI NEW YORK PA 233 SPRING STREET, NEW YORK, NY 10013, UNITED STATES BN 978-90-481-2468-8 PY 2009 BP 191 EP + DI 10.1007/978-90-481-2469-5_14 PG 3 WC Geochemistry & Geophysics; Environmental Sciences; Meteorology & Atmospheric Sciences SC Geochemistry & Geophysics; Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences GA BKP72 UT WOS:000268885100014 ER PT B AU Douglass, AR AF Douglass, Anne R. BE Zerefos, C Contopoulos, G Skalkeas, G TI Global Observations-The Key to Model Development and Improved Assessments SO TWENTY YEARS OF OZONE DECLINE LA English DT Proceedings Paper CT Symposium for the 20th Anniversary of the Montreal Protocol 2007 CY SEP, 2007 CL Athens, GREECE SP United Nat Environm Programme, Int Ozone Commiss, Acad Athens, Mariolopoulos-Kanaginis Fdn DE Constituent correlations; numerical transport; stratospheric constituents; stratospheric models ID CONSTITUENT TRANSPORT CALCULATIONS; NITROUS-OXIDE; TOTAL OZONE; STRATOSPHERE; CHEMISTRY; SCHEME AB The stratospheric models used to predict changes in the ozone due to changes in the atmospheric composition and climate have developed from the one-dimensional models of the 1970s to the three-dimensional models ill use today. Observations have played an obvious key role in model development, as they lead to the development and refinement of the conceptual model that underlies the computational model used in prediction. Observations also played another role. For example, a model failure to produce observed correlations between long-lived constituents in the lower stratosphere first led to an improvement in the numerical scheme transport algorithm and then inspired changes in the approach used to solve the equations of motion in a general circulation model. This led to improvements in several aspects of the simulation, including realistic propagation of the tape recorder signature in the tropical water vapor and a realistic distribution for lower stratospheric age-of-air. C1 NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Douglass, AR (reprint author), NASA, Goddard Space Flight Ctr, Code 613-3, Greenbelt, MD 20771 USA. EM Anne.R.Douglass@nasa.gov RI Douglass, Anne/D-4655-2012 NR 32 TC 0 Z9 0 U1 0 U2 0 PU SPRINGER PI NEW YORK PA 233 SPRING STREET, NEW YORK, NY 10013, UNITED STATES BN 978-90-481-2468-8 PY 2009 BP 251 EP 259 DI 10.1007/978-90-481-2469-5_18 PG 9 WC Geochemistry & Geophysics; Environmental Sciences; Meteorology & Atmospheric Sciences SC Geochemistry & Geophysics; Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences GA BKP72 UT WOS:000268885100018 ER PT B AU Schoeberl, MR Rodriguez, JM AF Schoeberl, Mark R. Rodriguez, Jose M. BE Zerefos, C Contopoulos, G Skalkeas, G TI The Rise and Fall of Dynamical Theories of the Ozone Hole SO TWENTY YEARS OF OZONE DECLINE LA English DT Proceedings Paper CT Symposium for the 20th Anniversary of the Montreal Protocol 2007 CY SEP, 2007 CL Athens, GREECE SP United Nat Environm Programme, Int Ozone Commiss, Acad Athens, Mariolopoulos Kanaginis Fdn DE Antarctic lower stratosphere; observations ozone hole; ozone hole theory; TOMS ID ANTARCTIC TOTAL-OZONE; STRATOSPHERIC TEMPERATURE; SATELLITE MEASUREMENTS; DEPLETION; CHLORINE; STATION; TRENDS; VAPOR; HCL AB During the late 1980's the appearance of the rapid spring decrease in Antarctic stratospheric ozone (the ozone hole) produced a large number of hypotheses. The two main contenders were the chemical hypothesis involving unmeasured chemical reactions, and the dynamical hypothesis involving a potential systematic change in Antarctic circulation. The strong observed correlation between column ozone changes and lower stratospheric temperature trends gave weight to the dynamical theory. However, after pioneering ground based and aircraft observations, it became clear that the Antarctic circulation was not changing during the column ozone decrease period as predicted by the dynamical hypothesis. These same observations showed significant chemical changes in the Antarctic lower stratosphere, which, along with focused laboratory chemical measurements showed that a variation of the original the chemical hypothesis explained the ozone hole phenomena. C1 [Schoeberl, Mark R.; Rodriguez, Jose M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Schoeberl, MR (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. EM mark.r.schoeberl@nasa.gov RI Rodriguez, Jose/G-3751-2013 OI Rodriguez, Jose/0000-0002-1902-4649 NR 32 TC 0 Z9 0 U1 1 U2 3 PU SPRINGER PI NEW YORK PA 233 SPRING STREET, NEW YORK, NY 10013, UNITED STATES BN 978-90-481-2468-8 PY 2009 BP 263 EP + DI 10.1007/978-90-481-2469-5_19 PG 4 WC Geochemistry & Geophysics; Environmental Sciences; Meteorology & Atmospheric Sciences SC Geochemistry & Geophysics; Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences GA BKP72 UT WOS:000268885100019 ER PT S AU Davila, JM Gopalswamy, N Thompson, BJ AF Davila, Joseph M. Gopalswamy, Nat Thompson, Barbara J. BE Gopalswamy, N Webg, DF TI Universal processes in heliophysics SO UNIVERSAL HELIOPHYSICAL PROCESSES SE IAU Symposium Proceedings Series LA English DT Proceedings Paper CT 257th Symposium of the International-Astronomical-Union CY SEP 15-19, 2008 CL Ioannina, GREECE SP Int Astron Union, Univ Ioannina, Greek Minist Educ & Religious Affairs, Greek Minist Culture, Int Heliophys Year, NASA DE Sun: general; interplanetary medium; solar system: general AB The structure of the Universe is determined primarily by the interplay of gravity which is dominant in condensed objects, and the magnetic force which is dominant in the rarefied medium between condensed objects. Each of these forces orders the matter into a, set of characteristic structures each with the ability to store and release energy in response to changes in the external environment. For the most part, the storage and release of energy proceeds through a number of Universal Processes. The coordinated study of these processes in different settings provides a deeper understanding of the underlying physics governing Universal Processes in astrophysics. C1 [Davila, Joseph M.; Gopalswamy, Nat; Thompson, Barbara J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Davila, JM (reprint author), NASA, Goddard Space Flight Ctr, Code 670, Greenbelt, MD 20771 USA. EM Joseph.M.Davila@nasa.gov; Nat.Gopalswamy@nasa.gov; Barbara.J.Thompson@nasa.gov; Nat.Gopalswamy@nasa.gov RI Gopalswamy, Nat/D-3659-2012; Thompson, Barbara/C-9429-2012 NR 5 TC 1 Z9 1 U1 0 U2 1 PU CAMBRIDGE UNIV PRESS PI CAMBRIDGE PA THE PITT BUILDING, TRUMPINGTON ST, CAMBRIDGE CB2 1RP, CAMBS, ENGLAND SN 1743-9213 BN 978-0-521-88988-9 J9 IAU SYMP P SERIES JI IAU Symposium Proc. Series PY 2009 VL 4 IS 257 BP 11 EP 16 DI 10.1017/S1743921309029032 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BJH42 UT WOS:000265828300002 ER PT S AU Gopalswamy, N Akiyama, S Yashiro, S AF Gopalswamy, N. Akiyama, S. Yashiro, S. BE Gopalswamy, N Webg, DF TI Major solar flares without coronal mass ejections SO UNIVERSAL HELIOPHYSICAL PROCESSES SE IAU Symposium Proceedings Series LA English DT Proceedings Paper CT 257th Symposium of the International-Astronomical-Union CY SEP 15-19, 2008 CL Ioannina, GREECE SP Int Astron Union, Univ Ioannina, Greek Minist Educ & Religious Affairs, Greek Minist Culture, Int Heliophys Year, NASA DE coronal mass ejections (CMEs); flares; particle emission; radio radiation ID ASSOCIATION AB We examine the source properties of X-class soft X-ray flares that were not associated with coronal mass ejections (CMEs). All the Hares were associated with intense microwave bursts implying the production of high energy electrons. However, most (85%) of the flares were not associated with metric type III bursts, even though open field lines existed in all but two of the active regions. The X-class flares seem to be truly confined because there was no material ejection (thermal or nonthermal) away from the flaring region into space. C1 [Gopalswamy, N.; Akiyama, S.; Yashiro, S.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Gopalswamy, N (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. EM nat.gopalswamy@nasa.gov; sachiko.akiyama@nasa.gov; seiji.yashiro@nasa.gov RI Gopalswamy, Nat/D-3659-2012 NR 11 TC 3 Z9 3 U1 0 U2 2 PU CAMBRIDGE UNIV PRESS PI CAMBRIDGE PA THE PITT BUILDING, TRUMPINGTON ST, CAMBRIDGE CB2 1RP, CAMBS, ENGLAND SN 1743-9213 BN 978-0-521-88988-9 J9 IAU SYMP P SERIES JI IAU Symposium Proc. Series PY 2009 VL 4 IS 257 BP 283 EP 286 DI 10.1017/S174392130902941X PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BJH42 UT WOS:000265828300037 ER PT S AU MacDowall, RJ Richardson, IG Hess, RA Thejappa, G AF MacDowall, R. J. Richardson, I. G. Hess, R. A. Thejappa, G. BE Gopalswamy, N Webg, DF TI Re-examining the correlation of complex solar type III radio bursts and solar energetic particles SO UNIVERSAL HELIOPHYSICAL PROCESSES SE IAU Symposium Proceedings Series LA English DT Proceedings Paper CT 257th Symposium of the International-Astronomical-Union CY SEP 15-19, 2008 CL Ioannina, GREECE SP Int Astron Union, Univ Ioannina, Greek Minist Educ & Religious Affairs, Greek Minist Culture, Int Heliophys Year, NASA DE acceleration of particles; shock waves; Sun: radio radiation; Sun: coronal mass ejections (CMEs); Sun: flares ID ACCELERATION; ELECTRONS; EVENTS AB Interplanetary radio observations provide important information on particle acceleration processes at the Sun and propagation of the accelerated particles in the solar wind. Cane et al. (2002) have drawn attention to a, class of prominent radio bursts that accompany > 20 MeV solar proton events. They call these bursts 'type III-L' because: they are fast, drifting (like normal type III bursts associated with electrons accelerated at impulsive solar flares); they are Long-lasting compared to normal type III bursts: they occur Late compared to the onset of the related solar event; and, they commence at Lower frequencies (similar to 100 MHz) than normal type III bursts, suggesting that they originate higher in the corona at similar to 0.5 R(s) above the Sun. We report, on all analysis of the correlated radio and SEP events during 1996-2006 using the Wind Waves and near-Earth SEP data sets, and discuss whether the characteristics of the complex type III bursts (at less than 14 MHz) will permit them to serve as proxies for SEP event occurrence and intensity. C1 [MacDowall, R. J.; Richardson, I. G.; Hess, R. A.; Thejappa, G.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP MacDowall, RJ (reprint author), NASA, Goddard Space Flight Ctr, Code 695, Greenbelt, MD 20771 USA. EM robert.macdowall@nasa.gov; ian.g.richardson@nasa.gov; roger.hess@nasa.gov; thejappa.golla@nasa.gov RI MacDowall, Robert/D-2773-2012; Gopalswamy, Nat/D-3659-2012; OI Richardson, Ian/0000-0002-3855-3634 NR 11 TC 1 Z9 1 U1 0 U2 0 PU CAMBRIDGE UNIV PRESS PI CAMBRIDGE PA THE PITT BUILDING, TRUMPINGTON ST, CAMBRIDGE CB2 1RP, CAMBS, ENGLAND SN 1743-9213 BN 978-0-521-88988-9 J9 IAU SYMP P SERIES JI IAU Symposium Proc. Series PY 2009 VL 4 IS 257 BP 335 EP 340 DI 10.1017/S1743921309029512 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BJH42 UT WOS:000265828300046 ER PT S AU Grebowsky, JM Aikin, AC AF Grebowsky, Joseph M. Aikin, Arthur C. BE Gopalswamy, N Webg, DF TI Planetary ionospheres - sources and dynamic drivers SO UNIVERSAL HELIOPHYSICAL PROCESSES SE IAU Symposium Proceedings Series LA English DT Proceedings Paper CT 257th Symposium of the International-Astronomical-Union CY SEP 15-19, 2008 CL Ioannina, GREECE SP Int Astron Union, Univ Ioannina, Greek Minist Educ & Religious Affairs, Greek Minist Culture, Int Heliophys Year, NASA DE earth; meteors; meteoroids; planets and satellites: general; magnetic fields ID RADIO OCCULTATIONS; MARS; ATMOSPHERE; JUPITER; EUROPA; VENUS AB External energy inputs into all planetary tipper atmospheres (including more than a half dozen moons with atmospheres) are comprised of combinations of solar EUV, soft x-rays, solar energetic particles, solar wind charged particles, magnetospherically accelerated particles, solar wind electric field, interplanetary dust particles as well as propagating lower atmosphere disturbances. Each input, has analogous physical interactions with all planetary ionospheres and upper atmospheres, but the integrated consequences of the multiple energy inputs vary from planet to planet. The Earth forms the framework for most fundamental processes because of extensive measurements of the effects of each of the inputs. However the conditions at Earth are far different from those at the carbon dioxide atmosphere of magnetic field-free, slow-rotating Venus, the carbon dioxide atmosphere of Mars with patchy remnant magnetic fields, while the outer planets have hydrogen atmospheres, are fast rotating with intrinsic magnetic fields, and encompass moons that interact with the magnetospheres and have exotic atmospheres. Although the physical processes are known, our understanding of our solar system's ionospheres diminishes with increasing distance from the Sun. C1 [Grebowsky, Joseph M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Grebowsky, JM (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. EM joseph.m.grebowsky@nasa.gov; aaikin1@verizon.net RI Gopalswamy, Nat/D-3659-2012; Grebowsky, Joseph/I-7185-2013 NR 19 TC 0 Z9 0 U1 0 U2 1 PU CAMBRIDGE UNIV PRESS PI CAMBRIDGE PA THE PITT BUILDING, TRUMPINGTON ST, CAMBRIDGE CB2 1RP, CAMBS, ENGLAND SN 1743-9213 BN 978-0-521-88988-9 J9 IAU SYMP P SERIES JI IAU Symposium Proc. Series PY 2009 VL 4 IS 257 BP 499 EP 510 DI 10.1017/S1743921309029780 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BJH42 UT WOS:000265828300069 ER PT S AU Rankin, AL Huertas, A Matthies, LH AF Rankin, Arturo L. Huertas, Andres Matthies, Larry H. BE Gerhart, GR Gage, DW Shoemaker, CM TI Stereo vision based terrain mapping for off-road autonomous navigation SO UNMANNED SYSTEMS TECHNOLOGY XI SE Proceedings of SPIE LA English DT Proceedings Paper CT Conference on Unmanned Systems Technology XI CY APR 17-17, 2009 CL Orlando, FL SP SPIE DE Terrain mapping; stereo vision; passive perception; autonomous navigation ID MAP AB Successful off-road autonomous navigation by an unmanned ground vehicle (UGV) requires reliable perception and representation of natural terrain. While perception algorithms are used to detect driving hazards, terrain mapping algorithms are used to represent the detected hazards in a world model a UGV can use to plan safe paths. There are two primary ways to detect driving hazards with perception sensors mounted to a UGV: binary obstacle detection and traversability cost analysis. Binary obstacle detectors label terrain as either traversable or non-traversable, whereas, traversability cost analysis assigns a cost to driving over a discrete patch of terrain. In uncluttered environments where the non-obstacle terrain is equally traversable, binary obstacle detection is sufficient. However, in cluttered environments, some form of traversability cost analysis is necessary. The Jet Propulsion Laboratory (JPL) has explored both approaches using stereo vision systems. A set of binary detectors has been implemented that detect positive obstacles, negative obstacles, tree trunks, tree lines, excessive slope, low overhangs, and water bodies. A compact terrain map is built from each frame of stereo images. The mapping algorithm labels cells that contain obstacles as no-go regions, and encodes terrain elevation, terrain classification, terrain roughness, traversability cost, and a confidence value. The single frame maps are merged into a world map where temporal filtering is applied. In previous papers, we have described our perception algorithms that perform binary obstacle detection. In this paper, we summarize the terrain mapping capabilities that JPL has implemented during several UGV programs over the last decade and discuss some challenges to building terrain maps with stereo range data. C1 [Rankin, Arturo L.; Huertas, Andres; Matthies, Larry H.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Rankin, AL (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. NR 23 TC 5 Z9 5 U1 0 U2 6 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 978-0-8194-7598-5 J9 PROC SPIE PY 2009 VL 7332 AR 733210 DI 10.1117/12.819099 PG 17 WC Computer Science, Artificial Intelligence; Computer Science, Information Systems; Robotics; Optics SC Computer Science; Robotics; Optics GA BVS50 UT WOS:000292646300024 ER PT J AU Jones, JA Ciftcioglu, N Schmid, JF Barr, YR Griffith, D AF Jones, Jeffrey A. Ciftcioglu, Neva Schmid, Josef F. Barr, Yael R. Griffith, Donald TI Calcifying Nanoparticles (Nanobacteria): An Additional Potential Factor for Urolithiasis in Space Flight Crews SO UROLOGY LA English DT Article ID KIDNEY-STONE FORMATION; METABOLISM; CALCIUM; DISEASE AB Space flight-induced microgravity appears to be a risk factor for the development of urinary calculi, resulting in urolithiasis during and after spaceflight. Calcifying nanoparticles, or nanobacteria, multiply more rapidly in simulated microgravity and create external shells of calcium phosphate. The question arises whether calcifying nanoparticles are nidi for calculi and contribute to the development of clinically significant urolithiasis in those who are predisposed to the development Of urinary calculi because of intrinsic or extrinsic factors. This case report describes a calculus recovered after flight from an astronaut that, on morphologic and immunochemical analysis (including specific monoclonal antibody staining), demonstrated characteristics of calcifying nanoparticles. UROLOGY 73: 210.e11-210.e13, 2009. (C) 2009 Elsevier Inc. C1 [Jones, Jeffrey A.] NASA, Lyndon B Johnson Space Ctr, SD, Houston, TX 77058 USA. Baylor Coll Med, Houston, TX 77030 USA. Vet Affairs Med Ctr, Houston, TX 77030 USA. Univ Texas Med Branch, Galveston, TX USA. RP Jones, JA (reprint author), NASA, Lyndon B Johnson Space Ctr, SD, 2101 NASA Pkwy, Houston, TX 77058 USA. EM jeffrey.a.jones@nasa.gov NR 15 TC 5 Z9 6 U1 0 U2 6 PU ELSEVIER SCIENCE INC PI NEW YORK PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA SN 0090-4295 J9 UROLOGY JI Urology PD JAN PY 2009 VL 73 IS 1 AR 210.e11 DI 10.1016/j.urology.2008.01.033 PG 3 WC Urology & Nephrology SC Urology & Nephrology GA 393NJ UT WOS:000262379700054 PM 18718644 ER PT B AU Kouveliotou, C AF Kouveliotou, C. BE Stanek, KZ TI Bohdan Paczynski and Gamma-Ray Bursts SO VARIABLE UNIVERSE: A CELEBRATION OF BOHDAN PACZYNSKI SE ASTRONOMICAL SOCIETY OF THE PACIFIC CONFERENCE SERIES LA English DT Proceedings Paper CT Symposium on the Variable Universe - A Celebration of Bohdan Paczynski CY SEP 29-30, 2007 CL Princeton Univ, Princeton, NJ HO Princeton Univ ID EMISSION PROPERTIES; SPECTRAL CATALOG; HUBBLE DIAGRAM; RADIO; SUPERNOVAE; AFTERGLOW; BATSE; DISCOVERY; REDSHIFT; ORIGIN C1 NASA, George C Marshall Space Flight Ctr, NSSTC, Huntsville, AL 35805 USA. RP Kouveliotou, C (reprint author), NASA, George C Marshall Space Flight Ctr, NSSTC, 320 Sparkman Dr, Huntsville, AL 35805 USA. NR 63 TC 0 Z9 0 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 978-1-58381-682-0 J9 ASTR SOC P PY 2009 VL 403 BP 150 EP 170 PG 21 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BJC81 UT WOS:000264849400010 ER PT B AU Spera, DA AF Spera, David A. BE Spera, DA TI Introduction to Modern Wind Turbines SO WIND TURBINE TECHNOLOGY: FUNDAMENTAL CONCEPTS OF WIND TURBINE ENGINEERING, SECOND EDITION LA English DT Editorial Material; Book Chapter C1 [Spera, David A.] NASA, Wind Energy Projects, Glenn Res Ctr, Cleveland, OH USA. [Spera, David A.] DASCON Engn LLC, Bonita Springs, FL USA. RP Spera, DA (reprint author), DASCON Engn LLC, Bonita Springs, FL USA. NR 15 TC 2 Z9 2 U1 0 U2 0 PU AMER SOC MECHANICAL ENGINEERS PI NEW YORK PA THREE PARK AVENUE, NEW YORK, NY 10016-5990 USA BN 978-0-7918-0260-1 PY 2009 BP 47 EP 103 DI 10.1115/1.802601.ch2 D2 10.1115/1.802601 PG 57 WC Energy & Fuels; Engineering, Mechanical SC Energy & Fuels; Engineering GA BGT44 UT WOS:000324080100002 ER PT B AU Hubbard, HH Shepherd, KP AF Hubbard, Harvey H. Shepherd, Kevin P. BE Spera, DA TI Wind Turbine Acoustics SO WIND TURBINE TECHNOLOGY: FUNDAMENTAL CONCEPTS OF WIND TURBINE ENGINEERING, SECOND EDITION LA English DT Article; Book Chapter ID NOISE C1 [Hubbard, Harvey H.; Shepherd, Kevin P.] NASA Langley Res Ctr, Hampton, VA USA. RP Hubbard, HH (reprint author), NASA Langley Res Ctr, Hampton, VA USA. NR 61 TC 0 Z9 0 U1 0 U2 0 PU AMER SOC MECHANICAL ENGINEERS PI NEW YORK PA THREE PARK AVENUE, NEW YORK, NY 10016-5990 USA BN 978-0-7918-0260-1 PY 2009 BP 413 EP 465 DI 10.1115/1.802601.ch7 D2 10.1115/1.802601 PG 53 WC Energy & Fuels; Engineering, Mechanical SC Energy & Fuels; Engineering GA BGT44 UT WOS:000324080100009 ER PT B AU Thresher, RW Mirandy, LP Carne, TG Lobitz, DW James, GH AF Thresher, Robert W. Mirandy, Louis P. Carne, Thomas G. Lobitz, Donald W. James, George H., III BE Spera, DA TI Structural Dynamic Behavior of Wind Turbines SO WIND TURBINE TECHNOLOGY: FUNDAMENTAL CONCEPTS OF WIND TURBINE ENGINEERING, SECOND EDITION LA English DT Article; Book Chapter ID BLADE C1 [Thresher, Robert W.] Natl Renewable Energy Lab, Golden, CO USA. [Mirandy, Louis P.] GE Co, King Of Prussia, PA USA. [Carne, Thomas G.; Lobitz, Donald W.] Sandia Natl Labs, Albuquerque, NM 87185 USA. [James, George H., III] NASA Johnson Space Ctr, Houston, TX USA. RP Thresher, RW (reprint author), Natl Renewable Energy Lab, Golden, CO USA. NR 41 TC 0 Z9 0 U1 0 U2 0 PU AMER SOC MECHANICAL ENGINEERS PI NEW YORK PA THREE PARK AVENUE, NEW YORK, NY 10016-5990 USA BN 978-0-7918-0260-1 PY 2009 BP 605 EP 662 DI 10.1115/1.802601.ch11 D2 10.1115/1.802601 PG 58 WC Energy & Fuels; Engineering, Mechanical SC Energy & Fuels; Engineering GA BGT44 UT WOS:000324080100013 ER PT B AU Spera, DA AF Spera, David A. BE Spera, DA TI Fatigue Design of Wind Turbines SO WIND TURBINE TECHNOLOGY: FUNDAMENTAL CONCEPTS OF WIND TURBINE ENGINEERING, SECOND EDITION LA English DT Article; Book Chapter C1 [Spera, David A.] NASA, Wind Energy Projects, Glenn Res Ctr, Cleveland, OH USA. [Spera, David A.] DASCON Engn LLC, Bonita Springs, FL USA. RP Spera, DA (reprint author), DASCON Engn LLC, Bonita Springs, FL USA. NR 66 TC 0 Z9 0 U1 0 U2 0 PU AMER SOC MECHANICAL ENGINEERS PI NEW YORK PA THREE PARK AVENUE, NEW YORK, NY 10016-5990 USA BN 978-0-7918-0260-1 PY 2009 BP 663 EP 719 DI 10.1115/1.802601.ch12 D2 10.1115/1.802601 PG 57 WC Energy & Fuels; Engineering, Mechanical SC Energy & Fuels; Engineering GA BGT44 UT WOS:000324080100014 ER PT J AU Banks, ME McEwen, AS Kargel, JS Baker, VR Strom, RG Mellon, MT Gulick, VC Keszthelyi, L Herkenhoff, KE Pelletier, JD Jaeger, WL AF Banks, Maria E. McEwen, Alfred S. Kargel, Jeffrey S. Baker, Victor R. Strom, Robert G. Mellon, Michael T. Gulick, Virginia C. Keszthelyi, Laszlo Herkenhoff, Kenneth E. Pelletier, Jon D. Jaeger, Windy L. TI High Resolution Imaging Science Experiment (HiRISE) observations of glacial and periglacial morphologies in the circum-Argyre Planitia highlands, Mars SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Article ID ORBITER LASER ALTIMETER; NORTH-POLAR CAP; VALLES MARINERIS; ROCK GLACIERS; DEBRIS APRONS; ICE; DEPOSITS; HISTORY; WATER; FLOW AB The landscape of the Argyre Planitia and adjoining Charitum and Nereidum Montes in the southern hemisphere of Mars has been heavily modified since formation of the Argyre impact basin. This study examines morphologies in the Argyre region revealed in images acquired by the High Resolution Imaging Science Experiment ( HiRISE) camera and discusses the implications for glacial and periglacial processes. Distinctive features such as large grooves, semicircular embayments in high topography, and streamlined hills are interpreted as glacially eroded grooves, cirques, and whalebacks or roche moutonnee, respectively. Large boulders scattered across the floor of a valley may be ground moraine deposited by ice ablation. Glacial interpretations are supported by the association of these features with other landforms typical of glaciated landscapes such as broad valleys with parabolic cross sections and stepped longitudinal profiles, lobate debris aprons interpreted as remnant debris covered glaciers or rock glaciers, and possible hanging valleys. Aligned boulders observed on slopes may also indicate glacial processes such as fluting. Alternatively, boulders aligned on slopes and organized in clumps and polygonal patterns on flatter surfaces may indicate periglacial processes, perhaps postglaciation, that form patterned ground. At least portions of the Argyre region appear to have been modified by processes of ice accumulation, glacial flow, erosion, sediment deposition, ice stagnation and ablation, and perhaps subsequent periglacial processes. The type of bedrock erosion apparent in images suggests that glaciers were, at times, wet based. The number of superposed craters is consistent with geologically recent glacial activity, but may be due to subsequent modification. C1 [Banks, Maria E.; Pelletier, Jon D.] Univ Arizona, Dept Geosci, Tucson, AZ 85721 USA. [McEwen, Alfred S.; Strom, Robert G.] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA. [Kargel, Jeffrey S.; Baker, Victor R.] Univ Arizona, Dept Hydrol & Water Resources, Tucson, AZ 85721 USA. [Mellon, Michael T.] Univ Colorado, Lab Atmospher & Space Phys, Boulder, CO 80309 USA. [Gulick, Virginia C.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Gulick, Virginia C.] SETI Inst, Moffett Field, CA 94035 USA. [Keszthelyi, Laszlo; Herkenhoff, Kenneth E.; Jaeger, Windy L.] USGS, Astrogeol Team, Flagstaff, AZ 86001 USA. RP Banks, ME (reprint author), Univ Arizona, Dept Geosci, 1040 E 4th St, Tucson, AZ 85721 USA. EM mbanks@email.arizona.edu RI Mellon, Michael/C-3456-2016 FU NASA FX We gratefully acknowledge the invaluable assistance of the entire HiRISE team, including the software developers, the uplink and downlink teams, and the science team. This paper also benefited from detailed reviews by G. Komatsu and an anonymous reviewer. This work was supported by the NASA Mars Reconnaissance Orbiter project managed through the California Institute of Technology's Jet Propulsion Laboratory. NR 86 TC 26 Z9 26 U1 2 U2 11 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9097 J9 J GEOPHYS RES-PLANET JI J. Geophys. Res.-Planets PD DEC 31 PY 2008 VL 113 IS E12 AR E12015 DI 10.1029/2007JE002994 PG 20 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 390OC UT WOS:000262172600001 ER PT J AU Hashimoto, GL Roos-Serote, M Sugita, S Gilmore, MS Kamp, LW Carlson, RW Baines, KH AF Hashimoto, George L. Roos-Serote, Maarten Sugita, Seiji Gilmore, Martha S. Kamp, Lucas W. Carlson, Robert W. Baines, Kevin H. TI Felsic highland crust on Venus suggested by Galileo Near-Infrared Mapping Spectrometer data SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Article ID RADAR REFLECTIVITY; DEEP ATMOSPHERE; LANDING SITES; SURFACE; WATER; NIGHTSIDE; EARTH; REFLECTANCE; MAGELLAN; CLIMATE AB We evaluated the spatial variation of Venusian surface emissivity at 1.18 mu m wavelength and that of near-surface atmospheric temperature using multispectral images obtained by the Near-Infrared Mapping Spectrometer (NIMS) on board the Galileo spacecraft. The Galileo NIMS observed the nightside thermal emission from the surface and the deep atmosphere of Venus, which is attenuated by scattering from the overlying clouds. To analyze the NIMS data, we used a radiative transfer model based on the adding method. Although there is still an uncertainty in the results owing to the not well known parameters of the atmosphere, our analysis revealed that the horizontal temperature variation in the near-surface atmosphere is no more than +/- 2 K on the Venusian nightside and also suggests that the majority of lowlands likely has higher emissivity compared to the majority of highlands. One interpretation for the latter result is that highland materials are generally composed of felsic rocks. Since formation of a large body of granitic magmas requires water, the presence of granitic terrains would imply that Venus may have had an ocean and a mechanism to recycle water into the mantle in the past. C1 [Hashimoto, George L.] Kobe Univ, Org Adv Sci & Technol, Lab Earth & Planetary Atmospher Sci, Nada Ku, Kobe, Hyogo 6578501, Japan. [Kamp, Lucas W.; Carlson, Robert W.; Baines, Kevin H.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Gilmore, Martha S.] Wesleyan Univ, Dept Earth & Environm Sci, Middletown, CT 06459 USA. [Roos-Serote, Maarten] Lisbon Astron Observ, P-1349018 Lisbon, Portugal. [Sugita, Seiji] Univ Tokyo, Grad Sch Frontier Sci, Dept Complex Sci & Engn, Chiba 2778561, Japan. RP Hashimoto, GL (reprint author), Kobe Univ, Org Adv Sci & Technol, Lab Earth & Planetary Atmospher Sci, Nada Ku, 1-1 Rokkodai, Kobe, Hyogo 6578501, Japan. EM george@kobe-u.ac.jp; maarten@lightcurvefilms.com; sugita@k.u-tokyo.ac.jp; mgilmore@wesleyan.edu; lwk@mipl.jpl.nasa.gov; rcarlson@lively.jpl.nasa.gov; kbaines@scn.jpl.nasa.gov RI Gilmore, Martha/G-5856-2011; HASHIMOTO, George/B-1529-2011 FU Ministry of Education, Culture, Sports, Science and Technology (MEXT); Portuguese FCT [PDCTE/FNU/49822/2003, BSAB/584/2006] FX The authors express their thanks to anonymous reviewers for their constructive comments on this manuscript. G. L. H. would like to thank Teruyuki Nakajima for detailed discussion of radiative transfer modeling, Naomoto Iwagami for helpful discussion of gas absorption, Yutaka Abe for fruitful discussion of early evolution of terrestrial planets, Yukari Tsutsumi for her help in developing computational code, and Constantine Tsang for his technical aid in preparing figures. G. L. H. and S. S. thank Grants-in-Aid for Scientific Research and The 21st Century COE Program of Origin and Evolution of Planetary Systems of Ministry of Education, Culture, Sports, Science and Technology (MEXT) for support. M. R. S. is supported by Portuguese FCT project PDCTE/FNU/49822/2003 and FCT scholarship BSAB/584/2006. NR 65 TC 28 Z9 28 U1 2 U2 10 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0148-0227 J9 J GEOPHYS RES-PLANET JI J. Geophys. Res.-Planets PD DEC 31 PY 2008 VL 113 AR E00B24 DI 10.1029/2008JE003134 PG 10 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 390NX UT WOS:000262172100001 ER PT J AU Andre, N Blanc, M Maurice, S Schippers, P Pallier, E Gombosi, TI Hansen, KC Young, DT Crary, FJ Bolton, S Sittler, EC Smith, HT Johnson, RE Baragiola, RA Coates, AJ Rymer, AM Dougherty, MK Achilleos, N Arridge, CS Krimigis, SM Mitchell, DG Krupp, N Hamilton, DC Dandouras, I Gurnett, DA Kurth, WS Louarn, P Srama, R Kempf, S Waite, HJ Esposito, LW Clarke, JT AF Andre, N. Blanc, M. Maurice, S. Schippers, P. Pallier, E. Gombosi, T. I. Hansen, K. C. Young, D. T. Crary, F. J. Bolton, S. Sittler, E. C. Smith, H. T. Johnson, R. E. Baragiola, R. A. Coates, A. J. Rymer, A. M. Dougherty, M. K. Achilleos, N. Arridge, C. S. Krimigis, S. M. Mitchell, D. G. Krupp, N. Hamilton, D. C. Dandouras, I. Gurnett, D. A. Kurth, W. S. Louarn, P. Srama, R. Kempf, S. Waite, H. J. Esposito, L. W. Clarke, J. T. TI IDENTIFICATION OF SATURN'S MAGNETOSPHERIC REGIONS AND ASSOCIATED PLASMA PROCESSES: SYNOPSIS OF CASSINI OBSERVATIONS DURING ORBIT INSERTION SO REVIEWS OF GEOPHYSICS LA English DT Review ID NEUTRAL MASS-SPECTROMETER; KILOMETRIC RADIATION; ROTATION PERIOD; SOLAR-WIND; IO TORUS; THERMAL PLASMA; ENCELADUS; RADIO; FIELD; DYNAMICS AB Saturn's magnetosphere is currently studied from the microphysical to the global scale by the Cassini-Huygens mission. During the first half of 2004, in the approach phase, remote sensing observations of Saturn's magnetosphere gave access to its auroral, radio, UV, energetic neutral atom, and dust emissions. Then, on 1 July 2004, Cassini Saturn orbit insertion provided us with the first in situ exploration of Saturn's magnetosphere since Voyager. To date, Saturn orbit insertion is the only Cassini orbit to have been described in common by all field and particle instruments. We use the comprehensive suite of magnetospheric and plasma science instruments to give a unified description of the large-scale structure of the magnetosphere during this particular orbit, identifying the different regions and their boundaries. These regions consist of the Saturnian ring system region 1, within 3 Saturn radii R-S)) and the cold plasma torus region 2, within 5-6 R-S) in the inner magnetosphere, a dynamic and extended plasma sheet region 3), and an outer high-latitude magnetosphere region 4, beyond 12-14 R-S). We compare these observations to those made at the time of the Voyager encounters. Then, we identify some of the dominant chemical characteristics and dynamical phenomena in each of these regions. The inner magnetosphere is characterized by the presence of the dominant plasma and neutral sources of the Saturnian system, giving birth to a very special magnetosphere dominated by water products. The extended plasma sheet, where the ring current resides, is a variable region with stretched magnetic field lines and contains a mixture of cold and hot plasma populations resulting from plasma transport processes. The outer high-latitude magnetosphere is characterized by a quiet magnetic field and an absence of plasma. Saturn orbit insertion observations enabled us to capture a snapshot of the large-scale structure of the Saturnian magnetosphere and of some of the main plasma processes operating in this complex environment. The analysis of the broad diversity of these interaction processes will be one of the main themes of magnetospheric and plasma science during the Cassini mission. C1 [Andre, N.] European Space Agcy, Res & Sci Support Dept, NL-2200 Noordwijk, Netherlands. [Dougherty, M. K.; Achilleos, N.; Arridge, C. S.] Univ London Imperial Coll Sci Technol & Med, Blackett Lab, London SW7 2BZ, England. [Smith, H. T.; Johnson, R. E.; Baragiola, R. A.] Univ Virginia, Engn Phys Program, Charlottesville, VA 22904 USA. [Smith, H. T.; Johnson, R. E.; Baragiola, R. A.] Univ Virginia, Dept Astron, Charlottesville, VA 22904 USA. [Blanc, M.; Maurice, S.; Schippers, P.; Pallier, E.; Dandouras, I.; Louarn, P.] Ctr Etud Spatiale Rayonnements, F-31028 Toulouse, France. [Young, D. T.; Crary, F. J.; Bolton, S.; Waite, H. J.] SW Res Inst, San Antonio, TX 78238 USA. [Clarke, J. T.] Boston Univ, Ctr Space Phys, Boston, MA 02215 USA. [Coates, A. J.] Univ Coll London, Mullard Space Sci Lab, Dorking RH5 6NT, Surrey, England. [Esposito, L. W.] Univ Colorado, LASP, Boulder, CO 80309 USA. [Gombosi, T. I.; Hansen, K. C.] Univ Michigan, Dept Atmospher Ocean & Space Sci, Ctr Space Environm Modeling, Ann Arbor, MI 48109 USA. [Gurnett, D. A.; Kurth, W. S.] Univ Iowa, Dept Phys & Astron, Iowa City, IA 52242 USA. [Hamilton, D. C.] Univ Maryland, Dept Phys, College Pk, MD 20742 USA. [Srama, R.; Kempf, S.] Max Planck Nucl Phys, D-69117 Heidelberg, Germany. [Rymer, A. M.; Krimigis, S. M.; Mitchell, D. G.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA. [Krupp, N.] Max Planck Inst Sonnensyst Forsch, D-37191 Katlenburg Lindau, Germany. [Sittler, E. C.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Andre, N (reprint author), European Space Agcy, Res & Sci Support Dept, Keplerlaan 1,POB 299, NL-2200 Noordwijk, Netherlands. EM nandre@rssd.esa.int RI Arridge, Christopher/A-2894-2009; Gombosi, Tamas/G-4238-2011; Achilleos, Nicholas/C-1647-2008; Hansen, Kenneth/F-3693-2011; Clarke, John/C-8644-2013; Coates, Andrew/C-2396-2008; Smith, Howard/H-4662-2016 OI Arridge, Christopher/0000-0002-0431-6526; Gombosi, Tamas/0000-0001-9360-4951; Dandouras, Iannis/0000-0002-7121-1118; KEMPF, SASCHA/0000-0001-5236-3004; Hamilton, Douglas/0000-0001-6103-8019; Achilleos, Nicholas/0000-0002-5886-3509; Kurth, William/0000-0002-5471-6202; Hansen, Kenneth/0000-0002-8502-1980; Coates, Andrew/0000-0002-6185-3125; Smith, Howard/0000-0003-3537-3360 FU Science and Technology Facilities Council [PP/D00084X/1] NR 119 TC 13 Z9 13 U1 3 U2 14 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 8755-1209 EI 1944-9208 J9 REV GEOPHYS JI Rev. Geophys. PD DEC 31 PY 2008 VL 46 IS 4 AR RG4008 DI 10.1029/2007RG000238 PG 22 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 390PF UT WOS:000262175500001 ER PT J AU Bozzolo, G Mosca, HO del Grosso, MF AF Bozzolo, G. Mosca, H. O. del Grosso, M. F. TI Surface structure and composition of Ni-Ti alloys and their influence on the temperature-dependent segregation behavior SO APPLIED SURFACE SCIENCE LA English DT Article DE Surface Segregation; Ni-Ti alloys; Computer simulation; Semi-empirical methods ID SHAPE-MEMORY ALLOY; OXIDATION BEHAVIOR; LAYER AB Atomistic modeling of segregation in Ni-Ti alloys is performed using the Bozzolo-Ferrante-Smith (BFS) method for alloys. It is found that Ti segregation to the surface decreases rapidly even for small increases in Ni concentration. A competing process is identified in the vicinity of surface defects, leading to excess Ti coverage of the exposed surface and the creation of Ti-covered pits. A simple explanation based on an atom-by-atom energy analysis is found to satisfactorily explain the observed effects. (C) 2008 Elsevier B.gV. All rights reserved. C1 [Bozzolo, G.] Ohio Aerosp Inst, Cleveland, OH 44142 USA. [Bozzolo, G.] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. [Mosca, H. O.; del Grosso, M. F.] UA Fis, Comis Nacl Energia Atom, San Martin, Argentina. [Mosca, H. O.; del Grosso, M. F.] FRG Pacheco, GCMM, UTN, Gral Pacheco, Argentina. RP Bozzolo, G (reprint author), Ohio Aerosp Inst, 22800 Cedar Point Rd, Cleveland, OH 44142 USA. EM GuillermoBozzolo@oai.org FU NASA Fundamental Aeronautics FX Fruitful discussions with N. Bozzolo are gratefully acknowledged. This work was partially sponsored by the NASA Fundamental Aeronautics NR 19 TC 2 Z9 2 U1 1 U2 4 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0169-4332 J9 APPL SURF SCI JI Appl. Surf. Sci. PD DEC 30 PY 2008 VL 255 IS 5 BP 3004 EP 3010 DI 10.1016/j.apsusc.2008.08.060 PG 7 WC Chemistry, Physical; Materials Science, Coatings & Films; Physics, Applied; Physics, Condensed Matter SC Chemistry; Materials Science; Physics GA 378CR UT WOS:000261299200078 ER PT J AU Jiang, X Li, QB Liang, MC Shia, RL Chahine, MT Olsen, ET Chen, LL Yung, YL AF Jiang, Xun Li, Qinbin Liang, Mao-Chang Shia, Run-Lie Chahine, Moustafa T. Olsen, Edward T. Chen, Luke L. Yung, Yuk L. TI Simulation of upper tropospheric CO2 from chemistry and transport models SO GLOBAL BIOGEOCHEMICAL CYCLES LA English DT Article ID CARBON-DIOXIDE; ATMOSPHERIC CO2; VARIABILITY; SENSITIVITY; SINKS; FLUX; PARAMETERIZATION; CONVECTION; TRACERS; GASES AB The California Institute of Technology/Jet Propulsion Laboratory two-dimensional (2-D), three-dimensional (3-D) GEOS-Chem, and 3-D MOZART- 2 chemistry and transport models (CTMs), driven respectively by NCEP2, GEOS-4, and NCEP1 reanalysis data, have been used to simulate upper tropospheric CO2 from 2000 to 2004. Model results of CO2 mixing ratios agree well with monthly mean aircraft observations at altitudes between 8 and 13 km ( Matsueda et al., 2002) in the tropics. The upper tropospheric CO2 seasonal cycle phases are well captured by the CTMs. Model results have smaller seasonal cycle amplitudes in the Southern Hemisphere compared with those in the Northern Hemisphere, which are consistent with the aircraft data. Some discrepancies are evident between the model and aircraft data in the midlatitudes, where models tend to underestimate the amplitude of CO2 seasonal cycle. Comparison of the simulated vertical profiles of CO2 between the different models reveals that the convection in the 3-D models is likely too weak in boreal winter and spring. Model sensitivity studies suggest that convection mass flux is important for the correct simulation of upper tropospheric CO2. C1 [Jiang, Xun; Li, Qinbin; Chahine, Moustafa T.; Olsen, Edward T.; Chen, Luke L.] CALTECH, Jet Prop Lab, Div Sci, Pasadena, CA 91109 USA. [Liang, Mao-Chang] Acad Sinica, Environm Res Ctr, Taipei 115, Taiwan. [Liang, Mao-Chang] Natl Cent Univ, Grad Inst Astron, Jhongli, Taiwan. [Liang, Mao-Chang; Shia, Run-Lie; Yung, Yuk L.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. RP Jiang, X (reprint author), CALTECH, Jet Prop Lab, Div Sci, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM xun@gps.caltech.edu RI Chem, GEOS/C-5595-2014 FU NASA [102438-01.01.01]; NSF [ATM-9903790]; NSC [96-2628-M-001-018] FX This work is performed at JPL under contract with NASA and is supported by project 102438-01.01.01. We thank J. Randerson for useful inputs and helpful comments, two anonymous reviewers, and C. L. Quere for helpful comments. Our special thanks to Bob Yantosca at Harvard University for the help on the GEOS-Chem model and to Peter Hess, Larry Horowitz, and Jean-Francois Lamar on the MOZART-2 model. R. L. Shia and Y. L. Yung are supported by NSF grant ATM-9903790. M. C. Liang also would like to acknowledge the support from an NSC grant 96-2628-M-001-018 to Academia Sinica. NR 48 TC 13 Z9 13 U1 1 U2 7 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0886-6236 EI 1944-9224 J9 GLOBAL BIOGEOCHEM CY JI Glob. Biogeochem. Cycle PD DEC 30 PY 2008 VL 22 IS 4 AR GB4025 DI 10.1029/2007GB003049 PG 11 WC Environmental Sciences; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Environmental Sciences & Ecology; Geology; Meteorology & Atmospheric Sciences GA 390MU UT WOS:000262169200001 ER PT J AU Su, H Jiang, JH Vane, DG Stephens, GL AF Su, Hui Jiang, Jonathan H. Vane, Deborah G. Stephens, Graeme L. TI Observed vertical structure of tropical oceanic clouds sorted in large-scale regimes SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article AB The CloudSat cloud water content (CWC) profiles are sorted by a number of large-scale parameters obtained from reanalysis and satellite observations, including 500 hPa vertical velocity, sea surface temperature and its gradient, surface divergence, precipitation, water vapor path, convective available potential energy and lower tropospheric static stability. The sorting is physics-based and phenomenon-oriented. We find different degrees of clustering of cloud vertical structure in various large-scale regimes. The dominant modes are the deep and shallow clouds with peak CWC above 7 km and below 2 km, respectively, corresponding to distinctly different large-scale regimes. A middle-level peak of CWC around 5-7 km is discernible associated with the large-scale conditions similar to the shallow clouds. This study provides the first quantitative and comprehensive view of tropical CWC distributions in large-scale regimes. These results offer insights into cloud parameterizations and serve as new observational metrics for evaluation of cloud simulations in models. Citation: Su, H., J. H. Jiang, D. G. Vane, and G. L. Stephens (2008), Observed vertical structure of tropical oceanic clouds sorted in large-scale regimes, Geophys. Res. Lett., 35, L24704, doi: 10.1029/2008GL035888. C1 [Su, Hui; Jiang, Jonathan H.; Vane, Deborah G.] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. [Stephens, Graeme L.] Colorado State Univ, Dept Atmospher Sci, Ft Collins, CO 80523 USA. RP Su, H (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. EM hui.su@jpl.nasa.gov FU JPL RTD FX We thank the JPL R&TD FY08 funding support, discussions with J. Teixeira and X. Huang, and helpful comments from the two reviewers. This work is conducted at the Jet Propulsion Laboratory, California Institute of Technology, under contract with NASA. NR 8 TC 25 Z9 27 U1 1 U2 7 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 DEC 27 PY 2008 VL 35 IS 24 AR L24704 DI 10.1029/2008GL035888 PG 6 WC Geosciences, Multidisciplinary SC Geology GA 388SW UT WOS:000262040500001 ER PT J AU Hamilton, VE Morris, RV Gruener, JE Mertzman, SA AF Hamilton, Victoria E. Morris, Richard V. Gruener, John E. Mertzman, Stanley A. TI Visible, near-infrared, and middle infrared spectroscopy of altered basaltic tephras: Spectral signatures of phyllosilicates, sulfates, and other aqueous alteration products with application to the mineralogy of the Columbia Hills of Gusev Crater, Mars SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Review ID THERMAL EMISSION-SPECTROSCOPY; REMOTE-SENSING APPLICATIONS; HAWAIIAN PALAGONITIC SOIL; MINI-TES EXPERIMENT; MAUNA-KEA VOLCANO; MARTIAN SURFACE; REFLECTANCE SPECTROSCOPY; MERIDIANI-PLANUM; MU-M; MOSSBAUER SPECTROMETER AB We studied visible to near-infrared (VNIR, 0.35-2.5 mu m) and middle infrared (MIR, 1800-250 cm(-1), also called thermal infrared and vibrational) spectra of basaltic tephras from Mauna Kea volcano that were altered under ambient, hydrothermal ( hydrolytic and acid sulfate), and dry heat conditions. Although models of MIR spectra of altered tephras generally produce fits whose quality is reduced compared to deconvolutions of primary lithologies, they successfully identify major alteration phases (cristobalite, oxide, phyllosilicate, and sulfate) except in palagonites. MIR spectra of the < 45 mu m fraction of all altered tephra samples exhibit an H2O peak at similar to 1640 cm(-1), but it cannot be used as an indicator of H2O content. This feature is present with band strengths > 1% in spectra of the 500-1000 mu m fraction only if phyllosilicates are present. Although Mauna Kea palagonitic tephra is considered a VNIR analog to Martian dust, comparison of MIR altered tephra spectra (< 45 mu m fraction) to dust spectra retrieved from Mars Global Surveyor and Mars Exploration Rover instruments do not provide good spectral matches. The best MIR match is a tephra that has a strong plagioclase feldspar transparency feature and was altered under dry, high-temperature, oxidizing conditions. This sample is not a VNIR analog and is not a process analog, but it emphasizes the mineralogical importance of plagioclase feldspar in Martian dust. No single tephra is a good spectral analog across the VNIR and MIR. We found no evidence for substantial sulfates or phyllosilicates in Mini-Thermal Emission Spectrometer (Mini-TES) spectra from Gusev Crater. C1 [Hamilton, Victoria E.] SW Res Inst, Boulder, CO 80302 USA. [Morris, Richard V.; Gruener, John E.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. [Mertzman, Stanley A.] Franklin & Marshall Coll, Dept Earth & Environm, Lancaster, PA 17604 USA. RP Hamilton, VE (reprint author), SW Res Inst, 1050 Walnut St,Suite 300, Boulder, CO 80302 USA. EM hamilton@boulder.swri.edu FU NASA's Mars Fundamental Research and Planetary Geology and Geophysics programs; NASA Mars Exploration Rover Project; NASA Mars Reconnaissance Orbiter (CRISM) Project; NASA Johnson Space Center FX We thank Joe Michalski for providing several phyllosilicate and silica phase spectra and Ray Arvidson and Patrick McGuire for calculation of the transmission spectrum of H2O vapor. Steve Ruff provided Mini-TES spectra of dust and rocks in Gusev Crater. Jim Gooding collected the samples from Puu Pohaku, and Doug Ming and Trevor Graff assisted with collection of samples from Puu Poliahu and Puu Waiau. Some VNIR spectra were acquired with an ASD spectrometer provided by Ray Arvidson. Funding to V. E. H. for this work was provided in part by NASA's Mars Fundamental Research and Planetary Geology and Geophysics programs. R. V. M. acknowledges support of the NASA Mars Exploration Rover Project, the NASA Mars Reconnaissance Orbiter (CRISM) Project, and the NASA Johnson Space Center. We thank Gregg Swayze and Steve Ruff for their careful and detailed reviews, which have resulted in clarifications and other improvements to the manuscript. NR 109 TC 20 Z9 20 U1 1 U2 11 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 DEC 27 PY 2008 VL 113 IS E12 AR E12S43 DI 10.1029/2007JE003049 PG 30 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 388UC UT WOS:000262043700001 ER PT J AU Galli, A Wurz, P Kallio, E Ekenback, A Holmstrom, M Barabash, S Grigoriev, A Futaana, Y Fok, MC Gunell, H AF Galli, A. Wurz, P. Kallio, E. Ekenback, A. Holmstrom, M. Barabash, S. Grigoriev, A. Futaana, Y. Fok, M. -C. Gunell, H. TI Tailward flow of energetic neutral atoms observed at Mars SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Article ID SOLAR-WIND INTERACTION; SUBSOLAR ENA JET; 1ST-ENA OBSERVATIONS; ASPERA-3 OBSERVATIONS; UPPER-ATMOSPHERE; CHARGE-EXCHANGE; EXPRESS MISSION; SPACE PLASMAS; HYDROGEN; DISTRIBUTIONS AB The ASPERA-3 experiment on Mars Express provides the first measurements of energetic neutral atoms (ENAs) from Mars. These measurements are used to study the global structure of the interaction of the solar wind with the Martian atmosphere. In this study we describe the tailward ENA flow observed at the nightside of Mars. After characterizing energy spectra of hydrogen ENA signals, we present composite images of the ENA intensities and compare them to theoretical predictions (empirical and MHD models). We find that the tailward flow of hydrogen ENAs is mainly generated by shocked solar wind protons. Despite intensive search, no oxygen ENAs above the instrument threshold are detected. The results challenge existing plasma models and constrain the hydrogen exospheric densities and atmospheric hydrogen and oxygen loss rates at low solar activity. C1 [Galli, A.; Wurz, P.] Univ Bern, Inst Phys, CH-3012 Bern, Switzerland. [Kallio, E.] Finnish Meteorol Inst, FIN-00101 Helsinki, Finland. [Ekenback, A.; Holmstrom, M.; Barabash, S.; Grigoriev, A.; Futaana, Y.] Inst Rymdfys, SE-98128 Kiruna, Sweden. [Fok, M. -C.] NASA, Goddard Space Flight Ctr, Geospace Phys Lab, Greenbelt, MD 20771 USA. [Gunell, H.] W Virginia Univ, Dept Phys, Morgantown, WV 26506 USA. RP Galli, A (reprint author), Univ Bern, Inst Phys, Sidlerstr 5, CH-3012 Bern, Switzerland. EM galli@space.unibe.ch; peter.wurz@space.unibe.ch RI Fok, Mei-Ching/D-1626-2012; Gunell, Herbert/D-5611-2013; Futaana, Yoshifumi/P-5899-2014; Kallio, Esa/F-9410-2014; OI Futaana, Yoshifumi/0000-0002-7056-3517; Kallio, Esa/0000-0002-9791-804X; Gunell, Herbert/0000-0001-5379-1158 FU Swiss National Science Foundation FX We thank Y. Ma and A. F. Nagy for providing the ion fluxes from their MHD model that we used to compute the ENA fluxes. This work is supported by the Swiss National Science Foundation. NR 33 TC 10 Z9 10 U1 0 U2 1 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 DEC 25 PY 2008 VL 113 IS E12 AR E12012 DI 10.1029/2008JE003139 PG 17 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 388UB UT WOS:000262043600001 ER PT J AU Haba, Y Liebmann, AC Fukumura, K Kunieda, H Tsuruta, S AF Haba, Yoshito Liebmann, Andrew C. Fukumura, Keigo Kunieda, Hideyo Tsuruta, Sachiko TI XMM-Newton Observations of NGC 4051: Temporal Flux and Spectral Variability during Transition to the Faintest Phase in NGC 4051 SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN LA English DT Article DE galaxies: active; galaxies: individual (NGC 4051); galaxies: Seyfert; X-rays: galaxies ID LINE SEYFERT-1 GALAXY; ULTRALUMINOUS INFRARED GALAXIES; DENSE MOLECULAR GAS; X-RAY-SPECTRUM; ACTIVE GALACTIC NUCLEI; STAR-FORMATION RATE; ASCA OBSERVATIONS; ACCRETION FLOW; BLACK-HOLE; SWAN SONG AB We report on the results from temporal and spectral analyses of NGC 4051 observed with XMM-Newton. The X-ray variabilities in the higher-flux states are well explained by the combination of a variable, direct power law and a temporally stable, absorbed component. In low-flux states, however, spectral variations are mainly due to flux changes of the absorbed component. Furthermore, when the source enters into the lowest-flux state, the absorbed component no longer appears. One promising interpretation is that part of the central emission region is covered by a temporally stable material, while the size of the emission region varies so as to produce a flux variation predominantly in direct power-law component. Once the emission region becomes smaller than the size of the absorber, however. the absorbed flux also begins to decrease. Finally, when the emission region is reduced sufficiently, both the direct and absorbed components disappear (i.e., "switched off" state). In this state, we found the signature of thermal emission, whose temperature of 0.8 keV is in agreement with the average value obtained from statistical analyses of Seyfert 2, galaxies with starburst activity. This could suggest that NGC 4051 possesses a nuclear starburst region. C1 [Haba, Yoshito; Kunieda, Hideyo] Nagoya Univ, Dept Phys, Chikusa Ku, Nagoya, Aichi 4648602, Japan. [Liebmann, Andrew C.; Tsuruta, Sachiko] Montana State Univ, Dept Phys, Bozeman, MT 59717 USA. [Fukumura, Keigo] NASA, Goddard Space Flight Ctr, Gravitat Astrophys Lab, Greenbelt, MD 20771 USA. RP Haba, Y (reprint author), Nagoya Univ, Dept Phys, Chikusa Ku, Furo Cho, Nagoya, Aichi 4648602, Japan. FU Ministry of Education, Culture, Sports, Science and Technology FX We are deeply grateful to the whole XMM-Newton team for building, launching, calibrating, and operating the spacecraft and instruments. We thank an anonymous referee for useful comments that make our presentations clearer and more meaningful. Y. H. is supported by a Grant-in-Aid for the 21st Century COE "The Origin of the Universe and Matter: Physical Elucidation of the Cosmic History" from the Ministry of Education, Culture, Sports, Science and Technology. NR 50 TC 1 Z9 1 U1 0 U2 0 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0004-6264 EI 2053-051X J9 PUBL ASTRON SOC JPN JI Publ. Astron. Soc. Jpn. PD DEC 25 PY 2008 VL 60 IS 6 BP 1257 EP 1266 DI 10.1093/pasj/60.6.1257 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 433ZJ UT WOS:000265244100006 ER PT J AU Wen, GY Marshak, A Cahalan, RF AF Wen, Guoyong Marshak, Alexander Cahalan, Robert F. TI Importance of molecular Rayleigh scattering in the enhancement of clear sky reflectance in the vicinity of boundary layer cumulus clouds SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID AEROSOL OPTICAL-THICKNESS; MODIS; PRODUCTS; TERRA; OCEAN; LAND; ATMOSPHERES; RETRIEVAL; TRANSPORT; DATASETS AB Clouds increase the complexity of atmospheric radiative transfer processes, particularly for aerosol retrievals in clear regions in the vicinity of clouds. This study focuses on identifying mechanisms responsible for the enhancement of nadir reflectance in clear regions in the vicinity of cumulus clouds and quantifies the relative importance of each mechanism. Using cloud optical properties and surface albedo derived from Advanced Spaceborne Thermal Emission and Reflection Radiometer (ASTER) and Moderate Resolution Imaging Spectroradiometer (MODIS), we performed extensive Monte Carlo simulations of radiative transfer in two cumulus scenes in a biomass burning region in Brazil. The results show that the scattering of radiation by clouds, followed by upward Rayleigh scattering by molecules above cloud top over clear gaps, is the dominant mechanism for the enhancement of visible reflectance in clear regions in boundary layer cumulus field over dark surfaces with aerosols trapped in the boundary layer. The Rayleigh scattering contributes similar to 80% and similar to 50% to the total enhancement for wavelengths 0.47 mu m (with aerosol optical thickness 0.2) and 0.66 mu m (with aerosol optical thickness 0.1), respectively. Out of the total contribution of molecular scattering, similar to 90% arises from the clear atmosphere above cloud top height. The mechanism is valid for a large range of aerosol optical thicknesses (up to 1 in this study) for 0.47 mu m, and for aerosol optical thickness up to 0.2 for 0.66 mu m. Our results provide a basis to develop simplifications for future aerosol remote sensing from satellite. C1 [Wen, Guoyong; Marshak, Alexander; Cahalan, Robert F.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Wen, Guoyong] Univ Maryland Baltimore Cty, Goddard Earth Sci & Technol Ctr, Baltimore, MD 21228 USA. RP Wen, GY (reprint author), NASA, Goddard Space Flight Ctr, Code 613-2, Greenbelt, MD 20771 USA. EM Guoyong.Wen-1@nasa.gov RI Marshak, Alexander/D-5671-2012; Cahalan, Robert/E-3462-2012 OI Cahalan, Robert/0000-0001-9724-1270 FU NASA GSFC [DE-AI02-95ER6I96I]; NASA's Radiation Sciences Program [921266] FX This research was supported by the Department of Energy (under grant DE-AI02-95ER6I96I to NASA GSFC) as part of the Atmospheric Radiation Measurement (ARM) program, by NASA's Radiation Sciences Program (under grant 921266), and we thank program manager Hal Maring. We thank J. Coakley, N. Loeb, L. Remer, and T. Varnai for useful discussions. The authors were greatly inspired by our colleague Yoram J. Kaufman in aerosol research. NR 35 TC 18 Z9 18 U1 0 U2 2 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD DEC 24 PY 2008 VL 113 AR D24207 DI 10.1029/2008JD010592 PG 10 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 388TG UT WOS:000262041500003 ER PT J AU Yang, FH Zhu, AX Ichii, K White, MA Hashimoto, H Nemani, RR AF Yang, Feihua Zhu, A-Xing Ichii, Kazuhito White, Michael A. Hashimoto, Hirofumi Nemani, Ramakrishna R. TI Assessing the representativeness of the AmeriFlux network using MODIS and GOES data SO JOURNAL OF GEOPHYSICAL RESEARCH-BIOGEOSCIENCES LA English DT Article ID LAND-SURFACE TEMPERATURE; GROSS PRIMARY PRODUCTION; SUPPORT VECTOR MACHINE; VEGETATION INDEXES; COMBINING MODIS; FLUXES; ECOSYSTEM; EVAPOTRANSPIRATION; VALIDATION; CARBON AB The AmeriFlux network of eddy covariance towers has played a critical role in the analysis of terrestrial water and carbon dynamics. It has been used to understand the general principles of ecosystem behaviors and to scale up those principles from sites to regions. To support the generalization from individual sites to large regions, it is essential that all major ecoregions in North America are represented in the AmeriFlux network. In this study, we examined the representativeness of the AmeriFlux network by comparing the climate and vegetation across the coterminous United States in 2004 with those at the AmeriFlux network in 2000-2004 on the basis of remote sensing products. We found that the AmeriFlux network generally captured the climatic and vegetation characteristics in the coterminous United States with under-representations in the Rocky Mountain evergreen needleleaf forest, the Sierra Nevada Mountains, the Sonora desert, the northern Great Plains, the Great Basin Desert, and New England. In terms of site representativeness, our analysis suggested that Indiana Morgan Monroe State Forest, Indiana, and Harvard Forest, Massachusetts, were among the forest sites with high representativeness extents; while Audubon Research Ranch, Arizona, and Sky Oaks Young Chaparral were among the nonforest sites with high representativeness extents. C1 [Yang, Feihua] Univ Wisconsin, Dept Geog, Madison, WI 53706 USA. [Yang, Feihua; Ichii, Kazuhito; Hashimoto, Hirofumi; Nemani, Ramakrishna R.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Ichii, Kazuhito] Fukushima Univ, Fac Symbiot Syst Sci, Fukushima 9601296, Japan. [White, Michael A.] Utah State Univ, Dept Watershed Sci, Logan, UT 84322 USA. [Hashimoto, Hirofumi] Calif State Univ, Div Sci & Environm Policy, Seaside, CA USA. [Zhu, A-Xing] Chinese Acad Sci, Inst Geog Sci & Nat Resources Res, State Key Lab Resources & Environm Informat Syst, Beijing, Peoples R China. RP Yang, FH (reprint author), Univ Wisconsin, Dept Geog, 426 Sci Hall,550 N Pk St, Madison, WI 53706 USA. EM feihuayang@wisc.edu RI Ichii, Kazuhito/D-2392-2010; OI Ichii, Kazuhito/0000-0002-8696-8084; White, Michael/0000-0002-0238-8913 FU Chinese Academy of Sciences International Partnership Project [CXTD-Z2005-1]; National Basic Research Program of China [2007CB407207]; Chinese Academy of Sciences; NASA New Investigator Program; EOS; REASON; Department of Energy; National Oceanic and Atmospheric Administration; National Aeronautics and Space Administration; National Science Foundation FX The funding from the Chinese Academy of Sciences International Partnership Project (Human Activities and Ecosystem Changes (project CXTD-Z2005-1)), National Basic Research Program of China (2007CB407207), and the Chinese Academy of Sciences through the One-Hundred Talents Program to A-Xing Zhu was appreciated. M. A. White was supported by the NASA New Investigator Program. NASA's Science Mission Directorate funded part of this research through EOS and REASON grants to RRN. The authors also thank John W. Norman, James E. Burt, David J. Page, and John W. William for inspirations of this research. AmeriFlux was funded by the Department of Energy, the National Oceanic and Atmospheric Administration, the National Aeronautics and Space Administration, and the National Science Foundation. Special thanks to all scientists and supporting staffs at AmeriFlux sites. NR 26 TC 8 Z9 8 U1 0 U2 13 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0148-0227 J9 J GEOPHYS RES-BIOGEO JI J. Geophys. Res.-Biogeosci. PD DEC 24 PY 2008 VL 113 IS G4 AR G04036 DI 10.1029/2007JG000627 PG 11 WC Environmental Sciences; Geosciences, Multidisciplinary SC Environmental Sciences & Ecology; Geology GA 388TS UT WOS:000262042700001 ER PT J AU Crooker, NU Kahler, SW Gosling, JT Lepping, RP AF Crooker, N. U. Kahler, S. W. Gosling, J. T. Lepping, R. P. TI Evidence in magnetic clouds for systematic open flux transport on the Sun SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article ID CORONAL MASS EJECTIONS; SOLAR-WIND; ELECTRONS; TOPOLOGY; DEPLETIONS; EVENTS AB Most magnetic clouds encountered by spacecraft at 1 AU display a mix of unidirectional suprathermal electrons signaling open field lines and counterstreaming electrons signaling loops connected to the Sun at both ends. Assuming the open fields were originally loops that underwent interchange reconnection with open fields at the Sun, we determine the sense of connectedness of the open fields found in 72 of 97 magnetic clouds identified by the Wind spacecraft in order to obtain information on the location and sense of the reconnection and resulting flux transport at the Sun. The true polarity of the open fields in each magnetic cloud was determined from the direction of the suprathermal electron flow relative to the magnetic field direction. Results indicate that the polarity of all open fields within a given magnetic cloud is the same 89% of the time, implying that interchange reconnection at the Sun most often occurs in only one leg of a flux rope loop, thus transporting open flux in a single direction, from a coronal hole near that leg to the foot point of the opposite leg. This pattern is consistent with the view that interchange reconnection in coronal mass ejections systematically transports an amount of open flux sufficient to reverse the polarity of the heliospheric field through the course of the solar cycle. Using the same electron data, we also find that the fields encountered in magnetic clouds are only a third as likely to be locally inverted as not. While one might expect inversions to be equally as common as not in flux rope coils, consideration of the geometry of spacecraft trajectories relative to the modeled magnetic cloud axes leads us to conclude that the result is reasonable. C1 [Crooker, N. U.] Boston Univ, Ctr Space Phys, Boston, MA 02215 USA. [Gosling, J. T.] Univ Colorado, Atmospher & Space Phys Lab, Boulder, CO 80303 USA. [Kahler, S. W.] USAF, Res Lab, Space Vehicles Directorate, Hanscom AFB, MA 01731 USA. [Lepping, R. P.] NASA, Goddard Space Flight Ctr, Space Weather Lab, Greenbelt, MD 20771 USA. RP Crooker, NU (reprint author), Boston Univ, Ctr Space Phys, Boston, MA 02215 USA. EM crooker@bu.edu FU NASA [NNG06GC18G] FX This paper is based upon work supported by NASA under grant NNG06GC18G. NR 20 TC 10 Z9 10 U1 0 U2 1 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0148-0227 J9 J GEOPHYS RES-SPACE JI J. Geophys. Res-Space Phys. PD DEC 24 PY 2008 VL 113 IS A12 AR A12107 DI 10.1029/2008JA013628 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 388UH UT WOS:000262044200001 ER PT J AU Morris, RV Klingelhofer, G Schroder, C Fleischer, I Ming, DW Yen, AS Gellert, R Arvidson, RE Rodionov, DS Crumpler, LS Clark, BC Cohen, BA Mccoy, TJ Mittlefehldt, DW Schmidt, ME de Souza, PA Squyres, SW AF Morris, R. V. Klingelhoefer, G. Schroeder, C. Fleischer, I. Ming, D. W. Yen, A. S. Gellert, R. Arvidson, R. E. Rodionov, D. S. Crumpler, L. S. Clark, B. C. Cohen, B. A. Mccoy, T. J. Mittlefehldt, D. W. Schmidt, M. E. de Souza, P. A., Jr. Squyres, S. W. TI Iron mineralogy and aqueous alteration from Husband Hill through Home Plate at Gusev Crater, Mars: Results from the Mossbauer instrument on the Spirit Mars Exploration Rover SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Article ID MARTIAN SOIL; SPECTROMETER; METEORITES; HEMATITE; ROCKS; DUST; PATHFINDER; VOLCANO; ANALOG AB Spirit's Mossbauer (MB) instrument determined the Fe mineralogy and oxidation state of 71 rocks and 43 soils during its exploration of the Gusev plains and the Columbia Hills (West Spur, Husband Hill, Haskin Ridge, northern Inner Basin, and Home Plate) on Mars. The plains are predominantly float rocks and soil derived from olivine basalts. Outcrops at West Spur and on Husband Hill have experienced pervasive aqueous alteration as indicated by the presence of goethite. Olivine-rich outcrops in a possible mafic/ultramafic horizon are present on Haskin Ridge. Relatively unaltered basalt and olivine basalt float rocks occur at isolated locations throughout the Columbia Hills. Basalt and olivine basalt outcrops are found at and near Home Plate, a putative hydrovolcanic structure. At least three pyroxene compositions are indicated by MB data. MB spectra of outcrops Barnhill and Torquas resemble palagonitic material and thus possible supergene aqueous alteration. Deposits of Fe3+-sulfate soil, located at Paso Robles, Arad, and Tyrone, are likely products of acid sulfate fumarolic and/or hydrothermal activity, possibly in connection with Home Plate volcanism. Hematite-rich outcrops between Home Plate and Tyrone (e. g., Montalva) may also be products of this aqueous activity. Low water-to-rock ratios (isochemical alteration) are implied during palagonite, goethite, and hematite formation because bulk chemical compositions are basaltic (SO3-free basis). High water-to-rock ratios (leaching) under acid sulfate conditions are implied for the high-SiO2 rock and soil in Eastern Valley and the float rock FuzzySmith, which has possible pyrite/marcasite as a hydrothermal alteration product. C1 [Morris, R. V.; Schroeder, C.; Ming, D. W.; Mittlefehldt, D. W.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. [Arvidson, R. E.] Washington Univ, Dept Earth & Planetary Sci, St Louis, MO 63130 USA. [Clark, B. C.] Lockheed Martin Corp, Littleton, CO 80127 USA. [Cohen, B. A.] NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA. [Crumpler, L. S.] New Mexico Museum Nat Hist & Sci, Albuquerque, NM 87104 USA. [de Souza, P. A., Jr.] CSIRO, Tasmanian ICT Ctr, Hobart, Tas 7000, Australia. [Klingelhoefer, G.; Fleischer, I.; Rodionov, D. S.] Johannes Gutenberg Univ Mainz, Inst Anorgan & Analyt Chem, D-55128 Mainz, Germany. [Gellert, R.] Univ Guelph, Dept Phys, Guelph, ON N1G 2W1, Canada. [Mccoy, T. J.; Schmidt, M. E.] Smithsonian Inst, Dept Mineral Sci, Washington, DC 20560 USA. [Squyres, S. W.] Cornell Univ, Dept Astron, Ithaca, NY 14853 USA. [Yen, A. S.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Rodionov, D. S.] Moscow Space Res Inst, Moscow 117810, Russia. RP Morris, RV (reprint author), NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. EM richard.v.morris@nasa.gov RI de Souza, Paulo/B-8961-2008; Schroder, Christian/B-3870-2009; Centre, TasICT/D-1212-2011 OI de Souza, Paulo/0000-0002-0091-8925; Schroder, Christian/0000-0002-7935-6039; FU NASA Mars Exploration Rover Project; NASA Johnson Space Center; German Space Agency [50QM 99022]; Technical University of Darmstadt; University of Mainz FX R. V. M. and D. W. M. acknowledge support of the NASA Mars Exploration Rover Project and the NASA Johnson Space Center. C. S. acknowledges support by an appointment to the NASA Postdoctoral Program at the Johnson Space Center, administered by Oak Ridge Associated Universities through a contract with NASA. The MER MIMOS II Mossbauer spectrometers were developed and built with funding provided by the German Space Agency under contract 50QM 99022 and with additional support from the Technical University of Darmstadt and the University of Mainz. A portion of the work described in this paper was conducted at the Jet Propulsion Laboratory, California Institute of Technology under a contract with NASA. We acknowledge the unwavering support, dedication, and attention to detail of JPL engineering and MER operations staff and the MER Athena Science Team. We thank D. Agresti and Brad Jolliff for thoughtful and detailed reviews of the manuscript. NR 63 TC 70 Z9 72 U1 2 U2 32 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 DEC 23 PY 2008 VL 113 IS E12 AR E12S42 DI 10.1029/2008JE003201 PG 43 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 388UA UT WOS:000262043500001 ER PT J AU van der Werf, GR Dempewolf, J Trigg, SN Randerson, JT Kasibhatla, PS Gigliof, L Murdiyarso, D Peters, W Morton, DC Collatz, GJ Dolman, AJ DeFries, RS AF van der Werf, G. R. Dempewolf, J. Trigg, S. N. Randerson, J. T. Kasibhatla, P. S. Gigliof, L. Murdiyarso, D. Peters, W. Morton, D. C. Collatz, G. J. Dolman, A. J. DeFries, R. S. TI Climate regulation of fire emissions and deforestation in equatorial Asia SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF AMERICA LA English DT Article DE climate change; feedbacks; biomass burning; Indonesia; global carbon cycle ID SOUTHEAST-ASIA; MODIS; VEGETATION; INDONESIA; PEAT; ALGORITHM; DATASET; BORNEO; POLICY; HAZE AB Drainage of peatlands and deforestation have led to large-scale fires in equatorial Asia, affecting regional air quality and global concentrations of greenhouse gases. Here we used several sources of satellite data with biogeochemical and atmospheric modeling to better understand and constrain fire emissions from Indonesia, Malaysia, and Papua New Guinea during 2000-2006. We found that average fire emissions from this region [128 +/- 51 (1 sigma) Tg carbon (C) year(-1), T = 1012] were comparable to fossil fuel emissions. In Borneo, carbon emissions from fires were highly variable, fluxes during the moderate 2006 El Nino more than 30 times greater than those during the 2000 La Nina (and with a 2000-2006 mean of 74 +/- 33 Tg C yr(-1)). Higher rates of forest loss and larger areas of peatland becoming vulnerable to fire in drought years caused a strong nonlinear relation between drought and fire emissions in southern Borneo. Fire emissions from Sumatra showed a positive linear trend, increasing at a rate of 8 Tg C year(-2) (approximately doubling during 2000-2006). These results highlight the importance of including deforestation in future climate agreements. They also imply that land manager responses to expected shifts in tropical precipitation may critically determine the strength of climate-carbon cycle feedbacks during the 21st century. C1 [van der Werf, G. R.; Dolman, A. J.] Vrije Univ Amsterdam, Fac Earth & Life Sci, NL-1081 HV Amsterdam, Netherlands. [Dempewolf, J.; Morton, D. C.] Univ Maryland, Dept Geog, College Pk, MD 20742 USA. [Trigg, S. N.] Cranfield Univ, Integrated Earth Syst Sci Inst, Cranfield MK43 0AL, Beds, England. [Randerson, J. T.] Univ Calif Irvine, Dept Earth Syst Sci, Irvine, CA 92697 USA. [Kasibhatla, P. S.] Duke Univ, Nicholas Sch Environm, Durham, NC 27708 USA. [Gigliof, L.] Sci Syst & Applicat Inc, Lanham, MD 20706 USA. [Murdiyarso, D.] JI CIFOR, Ctr Int Forestry Res, Bogor 16680, Indonesia. [Peters, W.] Univ Wageningen & Res Ctr, Dept Meteorol & Air Qual, NL-6700 AA Wageningen, Netherlands. [Collatz, G. J.] NASA, Goddard Space Flight Ctr, Hydrospher & Biospher Sci Lab, Greenbelt, MD 20771 USA. [DeFries, R. S.] Columbia Univ, Dept Ecol Evolut & Environm Biol, New York, NY 10027 USA. RP van der Werf, GR (reprint author), Vrije Univ Amsterdam, Fac Earth & Life Sci, NL-1081 HV Amsterdam, Netherlands. EM guido.van.der.werf@falw.vu.nl RI Peters, Wouter/B-8305-2008; Kasibhatla, Prasad/A-2574-2010; collatz, george/D-5381-2012; Morton, Douglas/D-5044-2012; Xiongfei, Zhao/G-7690-2015; van der Werf, Guido/M-8260-2016; OI Peters, Wouter/0000-0001-8166-2070; van der Werf, Guido/0000-0001-9042-8630; Kasibhatla, Prasad/0000-0003-3562-3737; Dolman, A.J./0000-0003-0099-0457 FU National Aeronautics and Space Administration [NNG05GD20G, NNG04GK49G, NNG04GD89G]; Netherlands Organization for Scientific Research FX This research was supported by National Aeronautics and Space Administration grants NNG05GD20G, NNG04GK49G, and NNG04GD89G. G.R.v.d.W. was supported by a Veni grant from the Netherlands Organization for Scientific Research. NR 38 TC 133 Z9 136 U1 5 U2 81 PU NATL ACAD SCIENCES PI WASHINGTON PA 2101 CONSTITUTION AVE NW, WASHINGTON, DC 20418 USA SN 0027-8424 J9 P NATL ACAD SCI USA JI Proc. Natl. Acad. Sci. U. S. A. PD DEC 23 PY 2008 VL 105 IS 51 BP 20350 EP 20355 DI 10.1073/pnas.0803375105 PG 6 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 388BP UT WOS:000261995600031 PM 19075224 ER PT J AU Abbott, B Abbott, R Adhikari, R Ajith, P Allen, B Allen, G Amin, R Anderson, SB Anderson, WG Arain, MA Araya, M Armandula, H Armor, P Aso, Y Aston, S Aufmuth, P Aulbert, C Babak, S Ballmer, S Bantilan, H Barish, BC Barker, C Barker, D Barr, B Barriga, P Barton, MA Bartos, I Bastarrika, M Bayer, K Betzwieser, J Beyersdorf, PT Bilenko, IA Billingsley, G Biswas, R Black, E Blackburn, K Blackburn, L Blair, D Bland, B Bodiya, TP Bogue, L Bork, R Boschi, V Bose, S Brady, PR Braginsky, VB Brau, JE Brinkmann, M Brooks, A Brown, DA Brunet, G Bullington, A Buonanno, A Burmeister, O Byer, RL Cadonati, L Cagnoli, G Camp, JB Cannizzo, J Cannon, K Cao, J Cardenas, L Casebolt, T Castaldi, G Cepeda, C Chalkley, E Charlton, P Chatterji, S Chelkowski, S Chen, Y Christensen, N Clark, D Clark, J Cokelaer, T Conte, R Cook, D Corbitt, T Coyne, D Creighton, JDE Cumming, A Cunningham, L Cutler, RM Dalrymple, J Danzmann, K Davies, G DeBra, D Degallaix, J Degree, M Dergachev, V Desai, S DeSalvo, R Dhurandhar, S Diaz, M Dickson, J Di Credico, A Dietz, A Donovan, F Dooley, KL Doomes, EE Drever, RWP Duke, I Dumas, JC Dupuis, RJ Dwyer, JG Echols, C Effler, A Ehrens, P Espinoza, E Etzel, T Evans, T Fairhurst, S Fan, Y Fazi, D Fehrmann, H Fejer, MM Finn, LS Flasch, K Fotopoulos, N Freise, A Frey, R Fricke, T Fritschel, P Frolov, VV Fyffe, M Garofoli, J Gholami, I Giaime, JA Giampanis, S Giardina, KD Goda, K Goetz, E Goggin, L Gonzalez, G Gossler, S Gouaty, R Grant, A Gras, S Gray, C Gray, M Greenhalgh, RJS Gretarsson, AM Grimaldi, F Grosso, R Grote, H Grunewald, S Guenther, M Gustafson, EK Gustafson, R Hage, B Hallam, JM Hammer, D Hanna, C Hanson, J Harms, J Harry, G Harstad, E Hayama, K Hayler, T Heefner, J Heng, IS Hennessy, M Heptonstall, A Hewitson, M Hild, S Hirose, E Hoak, D Hosken, D Hough, J Hughey, B Huttner, SH Ingram, D Ito, M Ivanov, A Johnson, B Johnson, WW Jones, DI Jones, G Jones, R Ju, L Kalmus, P Kalogera, V Kamat, S Kanner, J Kasprzyk, D Katsavounidis, E Kawabe, K Kawamura, S Kawazoe, F Kells, W Keppel, DG Khalili, FY Khan, R Khazanov, E Kim, C King, P Kissel, JS Klimenko, S Kokeyama, K Kondrashov, V Kopparapu, RK Kozak, D Kozhevatov, I Krishnan, B Kwee, P Lam, PK Landry, M Lang, MM Lantz, B Lazzarini, A Lei, M Leindecker, N Leonhardt, V Leonor, I Libbrecht, K Lin, H Lindquist, P Lockerbie, NA Lodhia, D Lormand, M Lu, P Lubinski, M Lucianetti, A Luck, H Machenschalk, B MacInnis, M Mageswaran, M Mailand, K Mandic, V Marka, S Marka, Z Markosyan, A Markowitz, J Maros, E Martin, I Martin, RM Marx, JN Mason, K Matichard, F Matone, L Matzner, R Mavalvala, N McCarthy, R McClelland, DE McGuire, SC McHugh, M McIntyre, G McIvor, G McKechan, D McKenzie, K Meier, T Melissinos, A Mendell, G Mercer, RA Meshkov, S Messenger, CJ Meyers, D Miller, J Minelli, J Mitra, S Mitrofanov, VP Mitselmakher, G Mittleman, R Miyakawa, O Moe, B Mohanty, S Moreno, G Mossavi, K MowLowry, C Mueller, G Mukherjee, S Mukhopadhyay, H Muller-Ebhardt, H Munch, J Murray, P Myers, E Myers, J Nash, T Nelson, J Newton, G Nishizawa, A Numata, K O'Dell, J Ogin, G O'Reilly, B O'Shaughnessy, R Ottaway, DJ Ottens, RS Overmier, H Owen, BJ Pan, Y Pankow, C Papa, MA Parameshwaraiah, V Patel, P Pedraza, M Penn, S Perreca, A Petrie, T Pinto, IM Pitkin, M Pletsch, HJ Plissi, MV Postiglione, F Principe, M Prix, R Quetschke, V Raab, F Rabeling, DS Radkins, H Rainer, N Rakhmanov, M Ramsunder, M Rehbein, H Reid, S Reitze, DH Riesen, R Riles, K Rivera, B Robertson, NA Robinson, C Robinson, EL Roddy, S Rodriguez, A Rogan, AM Rollins, J Romano, JD Romie, J Route, R Rowan, S Rudiger, A Ruet, L Russell, P Ryan, K Sakata, S Samidi, M de la Jordana, LS Sandberg, V Sannibale, V Saraf, S Sarin, P Sathyaprakash, BS Sato, S Saulson, PR Savage, R Savov, P Schediwy, SW Schilling, R Schnabel, R Schofield, R Schutz, BF Schwinberg, P Scott, SM Searle, AC Sears, B Seifert, F Sellers, D Sengupta, AS Shawhan, P Shoemaker, DH Sibley, A Siemens, X Sigg, D Sinha, S Sintes, AM Slagmolen, BJJ Slutsky, J Smith, JR Smith, MR Smith, ND Somiya, K Sorazu, B Stein, LC Stochino, A Stone, R Strain, KA Strom, DM Stuver, A Summerscales, TZ Sun, KX Sung, M Sutton, PJ Takahashi, H Tanner, DB Taylor, R Taylor, R Thacker, J Thorne, KA Thorne, KS Thuering, A Tinto, M Tokmakov, KV Torres, C Torrie, C Traylor, G Trias, M Tyler, W Ugolini, D Ulmen, J Urbanek, K Vahlbruch, H Van Den Broeck, C van der Sluys, M Vass, S Vaulin, R Vecchio, A Veitch, J Veitch, P Villar, A Vorvick, C Vyachanin, SP Waldman, SJ Wallace, L Ward, H Ward, R Weinert, M Weinstein, A Weiss, R Wen, S Wette, K Whelan, JT Whitcomb, SE Whiting, BF Wilkinson, C Willems, PA Williams, HR Williams, L Willke, B Wilmut, I Winkler, W Wipf, CC Wiseman, AG Woan, G Wooley, R Worden, J Wu, W Yakushin, I Yamamoto, H Yan, Z Yoshida, S Zanolin, M Zhang, J Zhang, L Zhao, C Zotov, N Zucker, M Zweizig, J AF Abbott, B. Abbott, R. Adhikari, R. Ajith, P. Allen, B. Allen, G. Amin, R. Anderson, S. B. Anderson, W. G. Arain, M. A. Araya, M. Armandula, H. Armor, P. Aso, Y. Aston, S. Aufmuth, P. Aulbert, C. Babak, S. Ballmer, S. Bantilan, H. Barish, B. C. Barker, C. Barker, D. Barr, B. Barriga, P. Barton, M. A. Bartos, I. Bastarrika, M. Bayer, K. Betzwieser, J. Beyersdorf, P. T. Bilenko, I. A. Billingsley, G. Biswas, R. Black, E. Blackburn, K. Blackburn, L. Blair, D. Bland, B. Bodiya, T. P. Bogue, L. Bork, R. Boschi, V. Bose, S. Brady, P. R. Braginsky, V. B. Brau, J. E. Brinkmann, M. Brooks, A. Brown, D. A. Brunet, G. Bullington, A. Buonanno, A. Burmeister, O. Byer, R. L. Cadonati, L. Cagnoli, G. Camp, J. B. Cannizzo, J. Cannon, K. Cao, J. Cardenas, L. Casebolt, T. Castaldi, G. Cepeda, C. Chalkley, E. Charlton, P. Chatterji, S. Chelkowski, S. Chen, Y. Christensen, N. Clark, D. Clark, J. Cokelaer, T. Conte, R. Cook, D. Corbitt, T. Coyne, D. Creighton, J. D. E. Cumming, A. Cunningham, L. Cutler, R. M. Dalrymple, J. Danzmann, K. Davies, G. DeBra, D. Degallaix, J. Degree, M. Dergachev, V. Desai, S. DeSalvo, R. Dhurandhar, S. Diaz, M. Dickson, J. Di Credico, A. Dietz, A. Donovan, F. Dooley, K. L. Doomes, E. E. Drever, R. W. P. Duke, I. Dumas, J-C Dupuis, R. J. Dwyer, J. G. Echols, C. Effler, A. Ehrens, P. Espinoza, E. Etzel, T. Evans, T. Fairhurst, S. Fan, Y. Fazi, D. Fehrmann, H. Fejer, M. M. Finn, L. S. Flasch, K. Fotopoulos, N. Freise, A. Frey, R. Fricke, T. Fritschel, P. Frolov, V. V. Fyffe, M. Garofoli, J. Gholami, I. Giaime, J. A. Giampanis, S. Giardina, K. D. Goda, K. Goetz, E. Goggin, L. Gonzalez, G. Gossler, S. Gouaty, R. Grant, A. Gras, S. Gray, C. Gray, M. Greenhalgh, R. J. S. Gretarsson, A. M. Grimaldi, F. Grosso, R. Grote, H. Grunewald, S. Guenther, M. Gustafson, E. K. Gustafson, R. Hage, B. Hallam, J. M. Hammer, D. Hanna, C. Hanson, J. Harms, J. Harry, G. Harstad, E. Hayama, K. Hayler, T. Heefner, J. Heng, I. S. Hennessy, M. Heptonstall, A. Hewitson, M. Hild, S. Hirose, E. Hoak, D. Hosken, D. Hough, J. Hughey, B. Huttner, S. H. Ingram, D. Ito, M. Ivanov, A. Johnson, B. Johnson, W. W. Jones, D. I. Jones, G. Jones, R. Ju, L. Kalmus, P. Kalogera, V. Kamat, S. Kanner, J. Kasprzyk, D. Katsavounidis, E. Kawabe, K. Kawamura, S. Kawazoe, F. Kells, W. Keppel, D. G. Khalili, F. Ya Khan, R. Khazanov, E. Kim, C. King, P. Kissel, J. S. Klimenko, S. Kokeyama, K. Kondrashov, V. Kopparapu, R. K. Kozak, D. Kozhevatov, I. Krishnan, B. Kwee, P. Lam, P. K. Landry, M. Lang, M. M. Lantz, B. Lazzarini, A. Lei, M. Leindecker, N. Leonhardt, V. Leonor, I. Libbrecht, K. Lin, H. Lindquist, P. Lockerbie, N. A. Lodhia, D. Lormand, M. Lu, P. Lubinski, M. Lucianetti, A. Lueck, H. Machenschalk, B. MacInnis, M. Mageswaran, M. Mailand, K. Mandic, V. Marka, S. Marka, Z. Markosyan, A. Markowitz, J. Maros, E. Martin, I. Martin, R. M. Marx, J. N. Mason, K. Matichard, F. Matone, L. Matzner, R. Mavalvala, N. McCarthy, R. McClelland, D. E. McGuire, S. C. McHugh, M. McIntyre, G. McIvor, G. McKechan, D. McKenzie, K. Meier, T. Melissinos, A. Mendell, G. Mercer, R. A. Meshkov, S. Messenger, C. J. Meyers, D. Miller, J. Minelli, J. Mitra, S. Mitrofanov, V. P. Mitselmakher, G. Mittleman, R. Miyakawa, O. Moe, B. Mohanty, S. Moreno, G. Mossavi, K. MowLowry, C. Mueller, G. Mukherjee, S. Mukhopadhyay, H. Mueller-Ebhardt, H. Munch, J. Murray, P. Myers, E. Myers, J. Nash, T. Nelson, J. Newton, G. Nishizawa, A. Numata, K. O'Dell, J. Ogin, G. O'Reilly, B. O'Shaughnessy, R. Ottaway, D. J. Ottens, R. S. Overmier, H. Owen, B. J. Pan, Y. Pankow, C. Papa, M. A. Parameshwaraiah, V. Patel, P. Pedraza, M. Penn, S. Perreca, A. Petrie, T. Pinto, I. M. Pitkin, M. Pletsch, H. J. Plissi, M. V. Postiglione, F. Principe, M. Prix, R. Quetschke, V. Raab, F. Rabeling, D. S. Radkins, H. Rainer, N. Rakhmanov, M. Ramsunder, M. Rehbein, H. Reid, S. Reitze, D. H. Riesen, R. Riles, K. Rivera, B. Robertson, N. A. Robinson, C. Robinson, E. L. Roddy, S. Rodriguez, A. Rogan, A. M. Rollins, J. Romano, J. D. Romie, J. Route, R. Rowan, S. Ruediger, A. Ruet, L. Russell, P. Ryan, K. Sakata, S. Samidi, M. de la Jordana, L. Sancho Sandberg, V. Sannibale, V. Saraf, S. Sarin, P. Sathyaprakash, B. S. Sato, S. Saulson, P. R. Savage, R. Savov, P. Schediwy, S. W. Schilling, R. Schnabel, R. Schofield, R. Schutz, B. F. Schwinberg, P. Scott, S. M. Searle, A. C. Sears, B. Seifert, F. Sellers, D. Sengupta, A. S. Shawhan, P. Shoemaker, D. H. Sibley, A. Siemens, X. Sigg, D. Sinha, S. Sintes, A. M. Slagmolen, B. J. J. Slutsky, J. Smith, J. R. Smith, M. R. Smith, N. D. Somiya, K. Sorazu, B. Stein, L. C. Stochino, A. Stone, R. Strain, K. A. Strom, D. M. Stuver, A. Summerscales, T. Z. Sun, K-X Sung, M. Sutton, P. J. Takahashi, H. Tanner, D. B. Taylor, R. Taylor, R. Thacker, J. Thorne, K. A. Thorne, K. S. Thuering, A. Tinto, M. Tokmakov, K. V. Torres, C. Torrie, C. Traylor, G. Trias, M. Tyler, W. Ugolini, D. Ulmen, J. Urbanek, K. Vahlbruch, H. Van Den Broeck, C. van der Sluys, M. Vass, S. Vaulin, R. Vecchio, A. Veitch, J. Veitch, P. Villar, A. Vorvick, C. Vyachanin, S. P. Waldman, S. J. Wallace, L. Ward, H. Ward, R. Weinert, M. Weinstein, A. Weiss, R. Wen, S. Wette, K. Whelan, J. T. Whitcomb, S. E. Whiting, B. F. Wilkinson, C. Willems, P. A. Williams, H. R. Williams, L. Willke, B. Wilmut, I. Winkler, W. Wipf, C. C. Wiseman, A. G. Woan, G. Wooley, R. Worden, J. Wu, W. Yakushin, I. Yamamoto, H. Yan, Z. Yoshida, S. Zanolin, M. Zhang, J. Zhang, L. Zhao, C. Zotov, N. Zucker, M. Zweizig, J. CA LIGO Sci Collaboration TI First joint search for gravitational-wave bursts in LIGO and GEO 600 data SO CLASSICAL AND QUANTUM GRAVITY LA English DT Article ID SCIENCE RUN; INVERSE PROBLEM; DETECTOR; GEO-600; ALGORITHM AB We present the results of the first joint search for gravitational-wave bursts by the LIGO and GEO 600 detectors. We search for bursts with characteristic central frequencies in the band 768-2048 Hz in the data acquired between 22 February and 23 March, 2005 (fourth LSC Science Run-S4). We discuss the inclusion of the GEO 600 data in the Waveburst-CorrPower pipeline that first searches for coincident excess power events without taking into account differences in the antenna responses or strain sensitivities of the various detectors. We compare the performance of this pipeline to that of the coherent Waveburst pipeline based on the maximum likelihood statistic. This likelihood statistic is derived from a coherent sum of the detector data streams that takes into account the antenna patterns and sensitivities of the different detectors in the network. We find that the coherent Waveburst pipeline is sensitive to signals of amplitude 30-50% smaller than the Waveburst-CorrPower pipeline. We perform a search for gravitational-wave bursts using both pipelines and find no detection candidates in the S4 data set when all four instruments were operating stably. C1 [Abbott, B.; Abbott, R.; Adhikari, R.; Anderson, S. B.; Araya, M.; Armandula, H.; Ballmer, S.; Barish, B. C.; Betzwieser, J.; Billingsley, G.; Black, E.; Blackburn, K.; Bork, R.; Boschi, V.; Brooks, A.; Cannon, K.; Cardenas, L.; Cepeda, C.; Chatterji, S.; Coyne, D.; DeSalvo, R.; Dupuis, R. J.; Echols, C.; Ehrens, P.; Espinoza, E.; Etzel, T.; Fazi, D.; Fricke, T.; Goggin, L.; Gustafson, E. K.; Heefner, J.; Ivanov, A.; Kells, W.; Keppel, D. G.; King, P.; Kondrashov, V.; Kozak, D.; Lazzarini, A.; Lei, M.; Libbrecht, K.; Lindquist, P.; Mageswaran, M.; Mailand, K.; Maros, E.; Marx, J. N.; Meshkov, S.; Meyers, D.; Miller, J.; Miyakawa, O.; Ogin, G.; Patel, P.; Pedraza, M.; Robertson, N. A.; Russell, P.; Samidi, M.; Sannibale, V.; Sears, B.; Sengupta, A. S.; Smith, M. R.; Stochino, A.; Tinto, M.; Tyler, W.; Vass, S.; Villar, A.; Waldman, S. J.; Wallace, L.; Ward, R.; Weinstein, A.; Whitcomb, S. E.; Willems, P. A.; Zhang, L.; Zweizig, J.] CALTECH, LIGO, Pasadena, CA 91125 USA. [Ajith, P.; Allen, B.; Aulbert, C.; Brinkmann, M.; Burmeister, O.; Fehrmann, H.; Gossler, S.; Grote, H.; Harms, J.; Hewitson, M.; Lueck, H.; Machenschalk, B.; Messenger, C. J.; Mossavi, K.; Mueller-Ebhardt, H.; Pletsch, H. J.; Prix, R.; Ruediger, A.; Schilling, R.; Schnabel, R.; Seifert, F.; Somiya, K.; Weinert, M.; Winkler, W.] Max Planck Inst Gravitat Phys, Albert Einstein Inst, D-30167 Hannover, Germany. [Allen, B.; Anderson, W. G.; Armor, P.; Biswas, R.; Brady, P. R.; Creighton, J. D. E.; Flasch, K.; Fotopoulos, N.; Hammer, D.; Moe, B.; Papa, M. A.; Siemens, X.] Univ Wisconsin, Milwaukee, WI 53201 USA. [Allen, G.; Bullington, A.; Byer, R. L.; Casebolt, T.; Clark, D.; DeBra, D.; Degree, M.; Fejer, M. M.; Hennessy, M.; Lantz, B.; Leindecker, N.; Lu, P.; Markosyan, A.] Stanford Univ, Stanford, CA 94305 USA. [Amin, R.; Giaime, J. A.; Gouaty, R.; Hanna, C.; Johnson, W. W.; Kissel, J. S.; Matichard, F.; Rodriguez, A.; Sung, M.] Louisiana State Univ, Baton Rouge, LA 70803 USA. [Arain, M. A.; Klimenko, S.; Lin, H.; Lucianetti, A.; Mercer, R. A.; Mitselmakher, G.; Ottens, R. S.; Pankow, C.; Quetschke, V.; Reitze, D. H.; Tanner, D. B.; Whiting, B. F.; Wu, W.] Univ Florida, Gainesville, FL 32611 USA. [Aso, Y.; Bartos, I.; Dwyer, J. G.; Kalmus, P.; Kamat, S.; Khan, R.; Marka, S.; Marka, Z.; Matone, L.; Rollins, J.] Columbia Univ, New York, NY 10027 USA. [Aston, S.; Cutler, R. M.; Hild, S.; Lodhia, D.; Perreca, A.; Robinson, E. L.; Vecchio, A.; Veitch, J.] Univ Birmingham, Birmingham B15 2TT, W Midlands, England. [Aufmuth, P.; Danzmann, K.; Hage, B.; Thuering, A.; Vahlbruch, H.] Leibniz Univ Hannover, D-30167 Hannover, Germany. [Babak, S.; Chen, Y.; Degallaix, J.; Gholami, I.; Krishnan, B.; Papa, M. A.; Sintes, A. M.; Somiya, K.; Takahashi, H.] Max Planck Inst Gravitat Phys, Albert Einstein Inst, D-14476 Golm, Germany. [Bantilan, H.; Christensen, N.] Carleton Coll, Northfield, MN 55057 USA. [Barker, C.; Barker, D.; Garofoli, J.; Guenther, M.; Ingram, D.; Johnson, B.; Kawabe, K.; Landry, M.; Lubinski, M.; Mendell, G.; Moreno, G.; Myers, J.; Parameshwaraiah, V.; Raab, F.; Radkins, H.; Rivera, B.; Sandberg, V.; Schwinberg, P.; Sigg, D.; Vorvick, C.; Wilkinson, C.; Worden, J.] LIGO Hanford Observ, Richland, WA 99352 USA. [Barr, B.; Barton, M. A.; Bastarrika, M.; Clark, J.; Cunningham, L.; Grant, A.; Heng, I. S.; Heptonstall, A.; Hough, J.; Huttner, S. H.; Jones, R.; Miller, J.; Murray, P.; Pitkin, M.; Reid, S.; Robertson, N. A.; Rowan, S.; Strain, K. A.; Woan, G.] Univ Glasgow, Glasgow G12 8QQ, Lanark, Scotland. [Barriga, P.; Dumas, J-C; Fan, Y.; Gras, S.; Zhao, C.] Univ Western Australia, Crawley, WA 6009, Australia. [Bayer, K.; Blackburn, L.; Bodiya, T. P.; Brunet, G.; Cao, J.; Corbitt, T.; Donovan, F.; Fritschel, P.; Goda, K.; Grimaldi, F.; Harry, G.; Hughey, B.; Katsavounidis, E.; Markowitz, J.; Mason, K.; Mavalvala, N.; Mittleman, R.; Ruet, L.; Sarin, P.; Shoemaker, D. H.; Smith, N. D.; Weiss, R.] MIT, LIGO, Cambridge, MA 02139 USA. [Beyersdorf, P. T.] San Jose State Univ, San Jose, CA 95192 USA. [Bilenko, I. A.; Braginsky, V. B.; Khalili, F. Ya; Mitrofanov, V. P.; Vyachanin, S. P.] Moscow MV Lomonosov State Univ, Moscow 119992, Russia. [Bogue, L.; Evans, T.; Frolov, V. V.; Fyffe, M.; Giaime, J. A.; Giardina, K. D.; Hanson, J.; Lormand, M.; O'Reilly, B.; Overmier, H.; Roddy, S.; Romie, J.; Sellers, D.; Sibley, A.; Stuver, A.; Thacker, J.; Traylor, G.; Yakushin, I.] LIGO Livingston Observ, Livingston, LA 70754 USA. [Bose, S.; Rogan, A. M.] Washington State Univ, Pullman, WA 99164 USA. [Brau, J. E.; Frey, R.; Leonor, I.] Univ Oregon, Eugene, OR 97403 USA. [Dalrymple, J.; Hirose, E.; Saulson, P. R.; Smith, J. R.] Syracuse Univ, Syracuse, NY 13244 USA. [Buonanno, A.; Kanner, J.; Pan, Y.] Univ Maryland, College Pk, MD 20742 USA. [Cadonati, L.] Univ Massachusetts, Amherst, MA 01003 USA. [Camp, J. B.; Cannizzo, J.; Numata, K.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Castaldi, G.; Pinto, I. M.; Principe, M.] Univ Sannio Benevento, I-82100 Benevento, Italy. [Charlton, P.] Charles Sturt Univ, Wagga Wagga, NSW 2678, Australia. [Chen, Y.; Savov, P.] CALTECH CaRT, Pasadena, CA 91125 USA. [Cokelaer, T.; Davies, G.; Fairhurst, S.; Jones, G.; McKechan, D.; Robinson, C.; Schutz, B. F.; Sutton, P. J.; Van Den Broeck, C.] Cardiff Univ, Cardiff CF24 3AA, Wales. [Conte, R.; Postiglione, F.] Univ Salerno, I-84084 Salerno, Italy. [Dergachev, V.; Goetz, E.; Gustafson, R.; Riles, K.; Zhang, J.] Univ Michigan, Ann Arbor, MI 48109 USA. [Desai, S.; Finn, L. S.; Kopparapu, R. K.; Lang, M. M.; Minelli, J.; O'Shaughnessy, R.; Thorne, K. A.] Penn State Univ, University Pk, PA 16802 USA. [Dhurandhar, S.; Mukhopadhyay, H.] Interuniv Ctr Astron & Astrophys, Pune 411007, Maharashtra, India. [Diaz, M.; Grosso, R.; Hayama, K.; Mohanty, S.; Mukherjee, S.; Romano, J. D.; Stone, R.] Univ Texas Brownsville & Texas Southmost Coll, Brownsville, TX 78520 USA. [Dickson, J.; Lam, P. K.; McClelland, D. E.; McKenzie, K.; Rabeling, D. S.; Scott, S. M.; Searle, A. C.; Slagmolen, B. J. J.] Australian Natl Univ, Canberra, ACT 0200, Australia. [Doomes, E. E.; McGuire, S. C.] Southern Univ, Baton Rouge, LA 70813 USA. [Doomes, E. E.; McGuire, S. C.] A & M Coll, Baton Rouge, LA 70813 USA. [Fricke, T.; Melissinos, A.] Univ Rochester, Rochester, NY 14627 USA. [Hayler, T.; O'Dell, J.; Wilmut, I.] Rutherford Appleton Lab, Didcot OX11 0QX, Oxon, England. [Gretarsson, A. M.; Zanolin, M.] Embry Riddle Aeronaut Univ, Prescott, AZ 86301 USA. [Hosken, D.; Munch, J.; Veitch, P.] Univ Adelaide, Adelaide, SA 5005, Australia. [Hosken, D.; Munch, J.; Veitch, P.] Univ Southampton, Southampton SO17 1BJ, Hants, England. [Kalogera, V.; Kanner, J.; Kim, C.] Northwestern Univ, Evanston, IL 60208 USA. [Kawamura, S.; Kokeyama, K.; Leonhardt, V.; Nishizawa, A.; Sakata, S.; Sato, S.] Natl Astron Observ Japan, Tokyo 1818588, Japan. [Khazanov, E.; Kozhevatov, I.] Inst Appl Phys, Nizhnii Novgorod 603950, Russia. [Lockerbie, N. A.] Univ Strathclyde, Glasgow G1 1XQ, Lanark, Scotland. [Mandic, V.] Univ Minnesota, Minneapolis, MN 55455 USA. [McIvor, G.] Univ Texas Austin, Austin, TX 78712 USA. [McHugh, M.] Loyola Univ, New Orleans, LA 70118 USA. [Penn, S.] Hobart & William Smith Coll, Geneva, NY 14456 USA. [Yoshida, S.] SE Louisiana Univ, Hammond, LA 70402 USA. [de la Jordana, L. Sancho; Sintes, A. M.; Trias, M.] Univ Illes Balears, E-07122 Palma de Mallorca, Spain. [Saraf, S.] Sonoma State Univ, Rohnert Pk, CA 94928 USA. [Summerscales, T. Z.] Andrews Univ, Berrien Springs, MI 49104 USA. [Ugolini, D.] Trinity Univ, San Antonio, TX 78212 USA. [Zotov, N.] Louisiana Tech Univ, Ruston, LA 71272 USA. RP Abbott, B (reprint author), CALTECH, LIGO, Pasadena, CA 91125 USA. EM i.heng@physics.gla.ac.uk RI Ward, Robert/I-8032-2014; Vecchio, Alberto/F-8310-2015; Mow-Lowry, Conor/F-8843-2015; Khan, Rubab/F-9455-2015; Ottaway, David/J-5908-2015; Postiglione, Fabio/O-4744-2015; Biswas, Rahul/H-7474-2016; Sigg, Daniel/I-4308-2015; Pinto, Innocenzo/L-3520-2016; Harms, Jan/J-4359-2012; Bartos, Imre/A-2592-2017; Frey, Raymond/E-2830-2016; Mitrofanov, Valery/D-8501-2012; Bilenko, Igor/D-5172-2012; Allen, Bruce/K-2327-2012; Chen, Yanbei/A-2604-2013; Barker, David/A-5671-2013; Fricke, Thomas/B-6885-2013; Zhao, Chunnong/C-2403-2013; Ju, Li/C-2623-2013; Pitkin, Matthew/I-3802-2013; Vyatchanin, Sergey/J-2238-2012; Khazanov, Efim/B-6643-2014; Lucianetti, Antonio/G-7383-2014; Khalili, Farit/D-8113-2012; Hild, Stefan/A-3864-2010; Schutz, Bernard/B-1504-2010; Rowan, Sheila/E-3032-2010; Strain, Kenneth/D-5236-2011; Raab, Frederick/E-2222-2011; Lueck, Harald/F-7100-2011; Kawazoe, Fumiko/F-7700-2011; Freise, Andreas/F-8892-2011; Kawabe, Keita/G-9840-2011; Finn, Lee Samuel/A-3452-2009; Lam, Ping Koy/A-5276-2008; McClelland, David/E-6765-2010; Martin, Iain/A-2445-2010 OI Veitch, John/0000-0002-6508-0713; Principe, Maria/0000-0002-6327-0628; Papa, M.Alessandra/0000-0002-1007-5298; Kanner, Jonah/0000-0001-8115-0577; Nishizawa, Atsushi/0000-0003-3562-0990; Zweizig, John/0000-0002-1521-3397; O'Shaughnessy, Richard/0000-0001-5832-8517; Aulbert, Carsten/0000-0002-1481-8319; Freise, Andreas/0000-0001-6586-9901; Whiting, Bernard F/0000-0002-8501-8669; Ward, Robert/0000-0001-5503-5241; Whelan, John/0000-0001-5710-6576; Fairhurst, Stephen/0000-0001-8480-1961; Boschi, Valerio/0000-0001-8665-2293; Matichard, Fabrice/0000-0001-8982-8418; Pinto, Innocenzo M./0000-0002-2679-4457; Minelli, Jeff/0000-0002-5330-912X; Sorazu, Borja/0000-0002-6178-3198; Hallam, Jonathan Mark/0000-0002-7087-0461; Vecchio, Alberto/0000-0002-6254-1617; Khan, Rubab/0000-0001-5100-5168; Postiglione, Fabio/0000-0003-0628-3796; Biswas, Rahul/0000-0002-0774-8906; Sigg, Daniel/0000-0003-4606-6526; Frey, Raymond/0000-0003-0341-2636; Stein, Leo/0000-0001-7559-9597; Allen, Bruce/0000-0003-4285-6256; Zhao, Chunnong/0000-0001-5825-2401; Pitkin, Matthew/0000-0003-4548-526X; Strain, Kenneth/0000-0002-2066-5355; Lueck, Harald/0000-0001-9350-4846; Finn, Lee Samuel/0000-0002-3937-0688; Lam, Ping Koy/0000-0002-4421-601X; McClelland, David/0000-0001-6210-5842; FU United States National Science Foundation for the construction and operation of the LIGO Laboratory; Science and Technology Facilities Council of the United Kingdom; Max-Planck-Society; State of Niedersachsen/Germany; Australian Research Council; Council of Scientific and Industrial Research of India; Istituto Nazionale di Fisica Nucleare of Italy; Spanish Ministerio de Educacion y Ciencia; Conselleria d'Economia; Hisenda i Innovacio of the Govern de les Illes Balears; 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; LIGO Laboratory [LIGO-P080008-B-Z] FX The authors gratefully acknowledge the support of the United States National Science Foundation for the construction and operation of the LIGO Laboratory and 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. The authors also gratefully acknowledge the support of the research by these agencies and by the Australian Research Council, the Council of Scientific and Industrial Research of India, the Istituto Nazionale di Fisica Nucleare of Italy, the Spanish Ministerio de Educacion y Ciencia, the Conselleria d'Economia, Hisenda i Innovacio of the Govern de les Illes Balears, 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-P080008-B-Z. NR 29 TC 19 Z9 19 U1 3 U2 14 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0264-9381 J9 CLASSICAL QUANT GRAV JI Class. Quantum Gravity PD DEC 21 PY 2008 VL 25 IS 24 AR 245008 DI 10.1088/0264-9381/25/24/245008 PG 21 WC Astronomy & Astrophysics; Physics, Multidisciplinary; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA 379GD UT WOS:000261383800008 ER PT J AU Hoskinson, AR Hershkowitz, N Ashpis, DE AF Hoskinson, A. R. Hershkowitz, N. Ashpis, D. E. TI Force measurements of single and double barrier DBD plasma actuators in quiescent air SO JOURNAL OF PHYSICS D-APPLIED PHYSICS LA English DT Article ID ATMOSPHERIC-PRESSURE; DISCHARGE PLASMA; SURFACE PLASMA; MECHANISMS; RESPONSES AB We present the results of our experimental measurements of how variations in the discharge geometry of surface-mounted dielectric barrier discharges (DBDs) affect the force transferred to atmospheric pressure air. Our studies include both single barrier plasma actuators (one electrode insulated) and double barrier plasma actuators (both electrodes insulated) operated in quiescent air. Stagnation probe measurements of the induced air flow and direct force measurements using an electronic balance show that, for both actuator types, parallel time-averaged forces increase as the high voltage electrode diameter decreases. For single barrier actuators, this increase is exponential rather than linear as previously reported in the literature. The data from the two measurement techniques are directly proportional to one another. When the variation of velocity and pressure on all sides of an actuator are considered, the techniques show quantitative agreement. C1 [Hoskinson, A. R.; Hershkowitz, N.] Univ Wisconsin, Dept Engn Phys, Madison, WI 53706 USA. [Ashpis, D. E.] NASA, Glenn Res Ctr Lewis Field, Cleveland, OH 44135 USA. RP Hoskinson, AR (reprint author), Univ Wisconsin, Dept Engn Phys, 1500 Engn Dr, Madison, WI 53706 USA. EM arhoskinson@wisc.edu; hershkowitz@engr.wisc.edu RI Hoskinson, Alan/F-9752-2013; OI Ashpis, David/0000-0003-4193-6174 FU NASA [NNX07AB84A]; Air Force Office of Scientific Research (AFOSR) [FA9550-07-1-0025] FX This work was supported by the NASA under Cooperative Agreement NNX07AB84A and the Air Force Office of Scientific Research (AFOSR) under grant FA9550-07-1-0025. The authors thank Dr Riccardo Bonazza for several helpful discussions regarding the stagnation probe calculations and Dr Jon Ahn for helpful suggestions about pressure sensor set up. NR 24 TC 34 Z9 36 U1 1 U2 10 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0022-3727 J9 J PHYS D APPL PHYS JI J. Phys. D-Appl. Phys. PD DEC 21 PY 2008 VL 41 IS 24 AR 245209 DI 10.1088/0022-3727/41/24/245209 PG 9 WC Physics, Applied SC Physics GA 379GC UT WOS:000261383700029 ER PT J AU Fischer, CF Rubin, RH Rodriguez, M AF Fischer, C. Froese Rubin, R. H. Rodriguez, M. TI Multiconfiguration Dirac-Hartree-Fock energy levels and transition probabilities for 3d(5) in Fe IV SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE atomic data; atomic processes ID IRON PROJECT; ATOMIC DATA; NEBULA; EXCITATION AB Multiconfiguration Dirac-Hartree-Fock electric quadrupole (E2) and magnetic dipole (M1) transition probabilities are reported for transitions between levels of 3d(5) in [Fe IV]. The accuracy of the ab initio energy levels and the agreement in the length and velocity forms of the line strength for the E2 transitions are used as indicators of accuracy. The present E2 and M1 transition probabilities are compared with earlier Breit-Pauli results and other theories. An extensive set of transition probabilities with indicators of accuracy are reported in Appendices A and B. Recommended values of A(E2) + A(M1) are listed in Appendix C. C1 [Fischer, C. Froese] Natl Inst Stand & Technol, Gaithersburg, MD 20899 USA. [Rubin, R. H.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Rubin, R. H.] Orion Enterprises, Moffett Field, CA 94035 USA. [Rubin, R. H.] Peking Univ, Kavli Inst Astron & Astrophys, Beijing 100871, Peoples R China. [Rodriguez, M.] Inst Nacl Astrofis Opt & Electr, Puebla 72000, Mexico. RP Fischer, CF (reprint author), Natl Inst Stand & Technol, Gaithersburg, MD 20899 USA. EM charlotte.fischer@nist.gov FU NASA [HST-AR-10973.01-A, NAS5-26555]; Mexican CONACYT [50359-F] FX Support for this publication was provided by NASA through programme number HST-AR-10973.01-A (PI RR) from the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, under NASA contract NAS5-26555. MR acknowledges support from Mexican CONACYT project 50359-F. NR 23 TC 8 Z9 8 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 DEC 21 PY 2008 VL 391 IS 4 BP 1828 EP 1837 DI 10.1111/j.1365-2966.2008.13997.x PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 382PD UT WOS:000261617000026 ER PT J AU Helling, C Ackerman, A Allard, F Dehn, M Hauschildt, P Homeier, D Lodders, K Marley, M Rietmeijer, F Tsuji, T Woitke, P AF Helling, Ch. Ackerman, A. Allard, F. Dehn, M. Hauschildt, P. Homeier, D. Lodders, K. Marley, M. Rietmeijer, F. Tsuji, T. Woitke, P. TI A comparison of chemistry and dust cloud formation in ultracool dwarf model atmospheres SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE stars: atmospheres; stars: low-mass; brown dwarfs ID LOW-MASS STARS; BROWN DWARFS; T-DWARFS; PHOTOSPHERIC ENVIRONMENT; CHEMICAL-COMPOSITION; CIRCUMSTELLAR DUST; PHOTOMETRIC SYSTEM; CONDENSATION; TEMPERATURE; ABUNDANCES AB The atmospheres of substellar objects contain clouds of oxides, iron, silicates and other refractory condensates. Water clouds are expected in the coolest objects. The opacity of these 'dust' clouds strongly affects both the atmospheric temperature-pressure profile and the emergent flux. Thus, any attempt to model the spectra of these atmospheres must incorporate a cloud model. However, the diversity of cloud models in atmospheric simulations is large and it is not always clear how the underlying physics of the various models compare. Likewise, the observational consequences of different modelling approaches can be masked by other model differences, making objective comparisons challenging. In order to clarify the current state of the modelling approaches, this paper compares five different cloud models in two sets of tests. Test case 1 tests the dust cloud models for a prescribed L-, L-T and T-dwarf atmospheric ( temperature T, pressure p, convective velocity v(conv)) structures. Test case 2 compares complete model atmosphere results for given ( effective temperature T(eff), surface gravity log g). All models agree on the global cloud structure but differ in opacity relevant details such as grain size, amount of dust, dust and gas-phase composition. These models can loosely be grouped into high- and low-altitude cloud models whereas the first appears generally redder in near-infrared colours than the latter. Comparisons of synthetic photometric fluxes translate into a modelling uncertainty in apparent magnitudes for our L-dwarf (T-dwarf) test case of 0.25 <= Delta m <= 0.875 (0.1 <= Delta m <= 1.375), taking into account the Two-Micron All Sky Survey, the UKIRT WFCAM, the Spitzer IRAC and VLT VISIR filters with UKIRT WFCAM being the most challenging for the models. Future developments will need closer links with laboratory astrophysics, and a consistent treatment of the cloud chemistry and turbulence. C1 [Helling, Ch.] Univ St Andrews, SUPA, Sch Phys & Astron, St Andrews KY16 9SS, Fife, Scotland. [Ackerman, A.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA. [Allard, F.] Univ Lyon, Ecole Normale Super Lyon, CNRS, Ctr Rech Astrophys Lyon,UMR5574, F-69634 Lyon, France. [Allard, F.] CNRS, Inst Astrophys Paris, UMR 7095, F-75014 Paris, France. [Dehn, M.; Hauschildt, P.] Hamburger Sternwarte, D-21029 Hamburg, Germany. [Homeier, D.] Univ Gottingen, Inst Astrophys, D-137077 Gottingen, Germany. [Lodders, K.] Washington Univ, Dept Earth & Planetary Sci, Planetary Chem Lab, St Louis, MO 63130 USA. [Marley, M.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Rietmeijer, F.] Univ New Mexico, Dept Earth & Planetary Sci, Albuquerque, NM 87131 USA. [Tsuji, T.] Univ Tokyo, Inst Astron, Tokyo 1810015, Japan. [Woitke, P.] Royal Observ, UK Astron Technol Ctr, Edinburgh EH9 3HJ, Midlothian, Scotland. RP Helling, C (reprint author), Univ St Andrews, SUPA, Sch Phys & Astron, St Andrews KY16 9SS, Fife, Scotland. EM Christiane.Helling@st-and.ac.uk RI Ackerman, Andrew/D-4433-2012; Marley, Mark/I-4704-2013; OI Ackerman, Andrew/0000-0003-0254-6253; Homeier, Derek/0000-0002-8546-9128 FU Lorentz Center of the University Leiden; Nederlandse Organisatie voor Wetenschappelijk Onderzoek; The Netherlands research School for Astronomy; Scottish University Physics Alliance and European Space Agency FX We thank the anonymous referee for the valuable report. ChH thanks Alkes Scholz and Soren Witte for helpful discussions on the manuscript. We thank the participants of the workshop From Brown Dwarfs to Planets: Chemistry and Cloud Formation which was supported by the Lorentz Center of the University Leiden, Nederlandse Organisatie voor Wetenschappelijk Onderzoek, The Netherlands research School for Astronomy, the Scottish University Physics Alliance and European Space Agency. NR 92 TC 96 Z9 97 U1 2 U2 5 PU WILEY-BLACKWELL PUBLISHING, INC PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD DEC 21 PY 2008 VL 391 IS 4 BP 1854 EP 1873 DI 10.1111/j.1365-2966.2008.13991.x PG 20 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 382PD UT WOS:000261617000028 ER PT J AU Rucinski, SM Matthews, JM Kuschnig, R Pojmanski, G Rowe, J Guenther, DB Moffat, AFJ Sasselov, D Walker, GAH Weiss, WW AF Rucinski, Slavek M. Matthews, Jaymie M. Kuschnig, Rainer Pojmanski, Grzegorz Rowe, Jason Guenther, David B. Moffat, Anthony F. J. Sasselov, Dimitar Walker, Gordon A. H. Weiss, Werner W. TI Photometric variability of the T Tauri star TW Hya on time-scales of hours to years SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE stars: pre-main-sequence; stars: variables: other ID SKY AUTOMATED SURVEY; HYDRAE ASSOCIATION; SOUTHERN-HEMISPHERE; VARIABLE-STARS; CATALOG; DISK; DISCOVERY; MEMBERS; CANDIDATE; QUARTER AB Microvariability & Oscillations of STars ( MOST) and All Sky Automated Survey (ASAS) observations have been used to characterize photometric variability of TW Hya on time-scales from a fraction of a day to 7.5 weeks and from a few days to 8 yr, respectively. The two data sets have very different uncertainties and temporal coverage properties and cannot be directly combined, nevertheless, they suggest a global variability spectrum with 'flicker-noise' properties, that is with amplitudes a alpha 1/root f, over >4 decades in frequency, in the range f = 0.0003-10 cd(-1). A 3.7 d period is clearly present in the continuous 11 d, 0.07 d time resolution, observations by MOST in 2007. Brightness extrema coincide with zero-velocity crossings in periodic (3.56 d) radial-velocity variability detected in contemporaneous spectroscopic observations of Setiawan et al. and interpreted as caused by a planet. The 3.56/3.7 d periodicity was entirely absent in the second, 4 times longer MOST run in 2008, casting doubt on the planetary explanation. Instead, a spectrum of unstable single periods within the range of 2-9 d was observed; the tendency of the periods to progressively shorten was well traced using the wavelet analysis. The evolving periodicities and the overall flicker-noise characteristics of the TW Hya variability suggest a combination of several mechanisms, with the dominant ones probably related to the accretion processes from the disc around the star. C1 [Rucinski, Slavek M.] Univ Toronto, Dept Astron & Astrophys, Toronto, ON M5S 3H4, Canada. [Matthews, Jaymie M.; Kuschnig, Rainer; Walker, Gordon A. H.] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada. [Pojmanski, Grzegorz] Warsaw Univ, Astron Observ, PL-00478 Warsaw, Poland. [Rowe, Jason] NASA Ames Res Pk, Moffett Field, CA 94035 USA. [Guenther, David B.] St Marys Univ, Inst Computat Astrophys, Dept Phys & Astron, Halifax, NS B3H 3C3, Canada. [Moffat, Anthony F. J.] Univ Montreal, Dept Phys, Montreal, PQ H3C 3J7, Canada. [Moffat, Anthony F. J.] Ctr Res Astrophys Quebec, Quebec City, PQ, Canada. [Sasselov, Dimitar] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Weiss, Werner W.] Univ Vienna, Inst Astron, A-1180 Vienna, Austria. RP Rucinski, SM (reprint author), Univ Toronto, Dept Astron & Astrophys, 50 St George St, Toronto, ON M5S 3H4, Canada. EM rucinski@astro.utoronto.ca FU Natural Sciences and Engineering Research Council of Canada; AFJM; FQRNT (Quebec); Canadian Space Agency; Austrian Space Agency; Austrian Science Fund; Polish Ministry of Science [N20300731/1328] FX The Natural Sciences and Engineering Research Council of Canada supports the research of DBG, JMM, AFJM and SMR. Additional support for AFJM comes from FQRNT (Quebec). RK is supported by the Canadian Space Agency and WWW is supported by the Austrian Space Agency and the Austrian Science Fund. GP acknowledges the research grant N20300731/1328 from Polish Ministry of Science.; Special thanks are extended to Ray Jayawardhana, Marten van Kerkwijk and Alexis Brandeker for very useful comments and to John Percy for an excellent review.; This research has made use of the SIMBAD data base, operated at CDS, Strasbourg, France and NASA's Astrophysics Data System ( ADS) Bibliographic Services. NR 34 TC 44 Z9 44 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 DEC 21 PY 2008 VL 391 IS 4 BP 1913 EP 1924 DI 10.1111/j.1365-2966.2008.14014.x PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 382PD UT WOS:000261617000033 ER PT J AU Maraschi, L Foschini, L Ghisellini, G Tavecchio, F Sambruna, RM AF Maraschi, L. Foschini, L. Ghisellini, G. Tavecchio, F. Sambruna, R. M. TI Testing the blazar spectral sequence: X-ray-selected blazars SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE radiation mechanisms: non-thermal; galaxies: active; galaxies: jets ID RADIO-LOUD QUASARS; BL LACERTAE OBJECTS; FLUX-DENSITY VARIATIONS; ACTIVE GALACTIC NUCLEI; MEDIUM-SENSITIVITY SURVEY; LINE SEYFERT-1 GALAXIES; BURST ALERT TELESCOPE; JET-DISK CONNECTION; LOW-ENERGY CUTOFFS; GAMMA-RAYS AB We present simultaneous optical and X-ray data from Swift for a sample of radio-loud flat-spectrum quasars selected from the Einstein Medium Sensitivity Survey (EMSS). We present also a complete analysis of Swift and INTEGRAL data on four blazars recently discussed as possibly challenging the trends of the hypothesized 'blazar spectral sequence'. The spectral energy distributions (SEDs) of all these objects are modelled in terms of a general theoretical scheme, applicable to all blazars, leading to an estimate of the jets' physical parameters. Our results show that, in the case of the EMSS broad line blazars, X-ray selection does not lead to find sources with synchrotron peaks in the UV/X-ray range, as was the case for X-ray-selected BL Lacs. Instead, for a wide range of radio powers all the sources with broad emission lines show similar SEDs, with synchrotron components peaking below the optical/UV range. The SED models suggest that the associated inverse Compton (IC) emission should peak below the GeV range, but could be detectable in some cases by the Fermi Gamma-ray Space Telescope. Of the remaining four 'anomalous' blazars, two highly luminous sources with broad lines, claimed to possibly emit synchrotron X-rays, are shown to be better described with IC models for their X-ray emission. For one source with weak emission lines ( a BL Lac object) a synchrotron peak in the soft X-ray range is confirmed, while for the fourth source, exhibiting narrow emission lines typical of narrow-line Seyfert 1 galaxies, no evidence of X-ray emission from a relativistic jet is found. We re-examine the standing and interpretation of the original 'blazar spectral sequence' and suggest that the photon ambient, in which the particle acceleration and emission occur, is likely the main factor determining the shape of the blazar SED. A connection between SED shape and jet power/luminosity can however result through the link between the mass and accretion rate of the central black hole and the radiative efficiency of the resulting accretion flow, thus involving at least two parameters. C1 [Maraschi, L.; Ghisellini, G.; Tavecchio, F.] Osserv Astron Brera, INAF, I-20100 Milan, Italy. [Foschini, L.] INAF IASF Bologna, I-40129 Bologna, Italy. [Sambruna, R. M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Maraschi, L (reprint author), Osserv Astron Brera, INAF, V Brera 28, I-20100 Milan, Italy. EM laura.maraschi@brera.inaf.it RI Foschini, Luigi/H-3833-2012; OI Foschini, Luigi/0000-0001-8678-0324; Ghisellini, Gabriele/0000-0002-0037-1974 FU Jet Propulsion Laboratory, California Institute of Technology; National Aeronautics and Space Administration; Alfred P. Sloan Foundation; Participating Institutions; National Science Foundation; US Department of Energy; Japanese Monbukagakusho; Max Planck Society; Higher Education Funding Council for England; American Museum of Natural History; Astrophysical Institute Potsdam; University of Basel; University of Cambridge; Case Western Reserve University; University of Chicago, Drexel University, Fermilab; Institute for Advanced Study; Japan Participation Group; Johns Hopkins University; Joint Institute for Nuclear Astrophysics; Kavli Institute for Particle Astrophysics and Cosmology; Korean Scientist Group; Chinese Academy of Sciences (LAMOST), Los Alamos National Laboratory; Max-Planck-Institute for Astronomy (MPIA); Max-Planck-Institute for Astrophysics (MPA); New Mexico State University; Ohio State University; University of Pittsburgh; University of Portsmouth; Princeton University; United States Naval Observatory; University of Washington; ASI/INAF [I/088/06/0] FX We acknowledge funding from ASI/INAF with contract I/088/06/0. NR 75 TC 29 Z9 29 U1 0 U2 0 PU WILEY-BLACKWELL PUBLISHING, INC PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD DEC 21 PY 2008 VL 391 IS 4 BP 1981 EP 1993 DI 10.1111/j.1365-2966.2008.14030.x PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 382PD UT WOS:000261617000040 ER PT J AU Hair, JW Hostetler, CA Cook, AL Harper, DB Ferrare, RA Mack, TL Welch, W Izquierdo, LR Hovis, FE AF Hair, Johnathan W. Hostetler, Chris A. Cook, Anthony L. Harper, David B. Ferrare, Richard A. Mack, Terry L. Welch, Wayne Izquierdo, Luis Ramos Hovis, Floyd E. TI Airborne High Spectral Resolution Lidar for profiling aerosol optical properties SO APPLIED OPTICS LA English DT Article ID SINGLE-FREQUENCY OPERATION; IODINE ABSORPTION FILTER; RAYLEIGH-MIE LIDAR; ND-YAG LASERS; RAMAN LIDAR; SCATTERING PROPERTIES; ATMOSPHERIC AEROSOLS; EXTINCTION; STABILIZATION; CALIBRATION AB A compact, highly robust airborne High Spectral Resolution Lidar (HSRL) that provides measurements of aerosol backscatter and extinction coefficients and aerosol depolarization at two wavelengths has been developed, tested, and deployed on nine field experiments (over 650 flight hours). A unique and advantageous design element of the HSRL system is the ability to radiometrically calibrate the instrument internally, eliminating any reliance on vicarious calibration from atmospheric targets for which aerosol loading must be estimated. This paper discusses the design of the airborne HSRL, the internal calibration and accuracy of the instrument, data products produced, and observations and calibration data from the first two field missions: the Joint Intercontinental Chemical Transport Experiment-Phase B (INTEX-B)/Megacity Aerosol Experiment-Mexico City (MAX-Mex)/Megacities Impacts on Regional and Global Environment (MILAGRO) field mission (hereafter MILAGRO) and the Gulf of Mexico Atmospheric Composition and Climate Study/Texas Air Quality Study II (hereafter GoMACCS/TexAQS II). (C) 2008 Optical Society of America C1 [Hair, Johnathan W.; Hostetler, Chris A.; Cook, Anthony L.; Harper, David B.; Ferrare, Richard A.] NASA, Langley Res Ctr, Hampton, VA 23681 USA. [Mack, Terry L.] Langley Res Ctr, Hampton, VA 23681 USA. [Welch, Wayne] Welch Mech Designs LLC, Havre De Grace, MD 21078 USA. [Izquierdo, Luis Ramos] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Hovis, Floyd E.] Fibertek Inc, Herndon, VA 20170 USA. RP Hair, JW (reprint author), NASA, Langley Res Ctr, Hampton, VA 23681 USA. EM johnathan.w.hair@nasa.gov FU NASA LaRC; NASA HQ Science Mission Directorate; NASA CALIPSO Project; U.S. Department of Energy's Atmospheric Science Program [DE-AI02-05ER63985]; NASA LaRC Research Services Directorate FX The authors thank the two reviewers for their detailed reviews that improved the manuscript. We also acknowledge the support of the NASA LaRC, NASA HQ Science Mission Directorate, and the NASA CALIPSO Project for funding the development of the HSRL instrument. The deployment of the HSRL in these field experiments were supported in part by the U.S. Department of Energy's Atmospheric Science Program (Office of Science, BER, Grant DE-AI02-05ER63985). We also acknowledge the aircraft flight support provided by personnel in the NASA LaRC Research Services Directorate. NR 44 TC 177 Z9 187 U1 3 U2 40 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 DEC 20 PY 2008 VL 47 IS 36 BP 6734 EP 6752 DI 10.1364/AO.47.006734 PG 19 WC Optics SC Optics GA 395AQ UT WOS:000262494800006 PM 19104525 ER PT J AU Kwiatkowska, EJ Franz, BA Meister, G McClain, CR Xiong, XX AF Kwiatkowska, Ewa J. Franz, Bryan A. Meister, Gerhard McClain, Charles R. Xiong, Xiaoxiong TI Cross calibration of ocean-color bands from Moderate Resolution Imaging Spectroradiometer on Terra platform SO APPLIED OPTICS LA English DT Article ID ON-ORBIT CALIBRATION; REFLECTIVE SOLAR BANDS; WATER-LEAVING RADIANCE; ATMOSPHERIC CORRECTION; POLARIZATION-SENSITIVITY; SPECTRAL REFLECTANCE; SEAWIFS; ALGORITHM; INSTRUMENT; SENSORS AB Ocean-color applications require maxi main uncertainties in blue-wavelength water-leaving radiances in oligotrophic ocean of approximately 5%. Water-leaving radiances from Moderate Resolution Imaging Spectroradiometer (MODIS) on the Terra satellite, however, exhibit temporal drift of the order of 15% as well as sensor changes in response versus scan and polarization sensitivity, which cannot be tracked by onboard calibrators. This paper introduces an instrument characterization approach that uses Earth-view data as a calibration source. The approach models the top of the atmosphere signal over ocean that the instrument is expected to measure, including its polarization, with water-leaving radiances coming from another well-calibrated global sensor. The cross calibration allows for significant improvement in derived MODIS-Terra ocean-color products, with largest changes in the blue wavelengths. (C) 2008 Optical Society of America C1 [Kwiatkowska, Ewa J.; Franz, Bryan A.; Meister, Gerhard; McClain, Charles R.] NASA, Goddard Space Flight Ctr, Ocean Biol Proc Grp, Greenbelt, MD 20771 USA. [Kwiatkowska, Ewa J.; Franz, Bryan A.] Sci Applicat Int Corp, Beltsville, MD 20705 USA. [Meister, Gerhard] Futuretech Corp, Greenbelt, MD 20770 USA. [Xiong, Xiaoxiong] NASA, Goddard Space Flight Ctr, Moderate Resolut Imaging Spectroradiometer Charac, Greenbelt, MD 20771 USA. RP Kwiatkowska, EJ (reprint author), NASA, Goddard Space Flight Ctr, Ocean Biol Proc Grp, Greenbelt, MD 20771 USA. EM ewa.kwiatkowska@gmail.com RI Franz, Bryan/D-6284-2012; Meister, Gerhard/F-7159-2012 OI Franz, Bryan/0000-0003-0293-2082; FU NASA Research Opportunities in Space and Earth Sciences (ROSES); validation solicitation funding FX This work was supported under the NASA Research Opportunities in Space and Earth Sciences (ROSES) 2006 calibration and validation solicitation funding. NR 45 TC 43 Z9 43 U1 1 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 DEC 20 PY 2008 VL 47 IS 36 BP 6796 EP 6810 DI 10.1364/AO.47.006796 PG 15 WC Optics SC Optics GA 395AQ UT WOS:000262494800012 PM 19104531 ER PT J AU Numata, K Camp, J AF Numata, Kenji Camp, Jordan TI Interferometric testbed for nanometer level stabilization of environmental motion over long time scales SO APPLIED OPTICS LA English DT Article AB We developed an interferometric testbed to stabilize environmental motions over time scales of several hours and a length scale of 1 m. Typically, thermal and seismic motions on the ground are larger than 1 mu m over these scales, affecting the precision of more sensitive measurements. To suppress such motions, we built an active stabilization system composed of interferometric sensors, a hexapod actuator, and a frequency-stabilized laser. With this stabilized testbed, environmental motions were Suppressed down to the nanometer level. This system will allow us to perform sensitive measurements, such as ground testing of the Laser Interferometer Space Antenna, in the presence of enviromental noise. (C) 2008 Optical Society of America C1 [Numata, Kenji] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Numata, Kenji; Camp, Jordan] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Numata, K (reprint author), Univ Maryland, Dept Astron, College Pk, MD 20742 USA. EM Kenji.Numata@nasa.gov NR 15 TC 6 Z9 6 U1 0 U2 4 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 DEC 20 PY 2008 VL 47 IS 36 BP 6832 EP 6841 DI 10.1364/AO.47.006832 PG 10 WC Optics SC Optics GA 395AQ UT WOS:000262494800015 PM 19104534 ER PT J AU Campbell, J AF Campbell, Joel TI Synthetic quadrature phase detector/demodulator for Fourier transform spectrometers SO APPLIED OPTICS LA English DT Article ID DEMODULATION AB A method is developed to demodulate (velocity correct) Fourier transform spectrometer data that are taken with an analog to digital converter that digitizes equally spaced in time. This method makes it possible to use simple low-cost, high-resolution audio digitizers to record high-quality data without the need For an event timer or quadrature laser hardware and makes it possible to use a metrology laser of any wavelength. The reduced parts count and simple implementation make it an attractive alternative in space-based applications when compared to previous methods such as the Brault algorithm. (C) 2008 Optical Society of America C1 NASA, Langley Res Ctr, Hampton, VA 23662 USA. RP Campbell, J (reprint author), NASA, Langley Res Ctr, MS 488, Hampton, VA 23662 USA. EM joel.f.campbell@nasa.gov NR 12 TC 5 Z9 6 U1 1 U2 1 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 DEC 20 PY 2008 VL 47 IS 36 BP 6889 EP 6894 DI 10.1364/AO.47.006889 PG 6 WC Optics SC Optics GA 395AQ UT WOS:000262494800023 PM 19104542 ER PT J AU MacTavish, CJ Ade, PAR Battistelli, ES Benton, S Bihary, R Bock, JJ Bond, JR Brevik, J Bryan, S Contaldi, CR Crill, BP Dore, O Fissel, L Golwala, SR Halpern, M Hilton, G Holmes, W Hristov, VV Irwin, K Jones, WC Kuo, CL Lange, AE Lawrie, C Martin, TG Mason, P Montroy, TE Netterfield, CB Riley, D Ruhl, JE Runyan, M Trangsrud, A Tucker, C Turner, A Viero, M Wiebe, D AF MacTavish, C. J. Ade, P. A. R. Battistelli, E. S. Benton, S. Bihary, R. Bock, J. J. Bond, J. R. Brevik, J. Bryan, S. Contaldi, C. R. Crill, B. P. Dore, O. Fissel, L. Golwala, S. R. Halpern, M. Hilton, G. Holmes, W. Hristov, V. V. Irwin, K. Jones, W. C. Kuo, C. L. Lange, A. E. Lawrie, C. Martin, T. G. Mason, P. Montroy, T. E. Netterfield, C. B. Riley, D. Ruhl, J. E. Runyan, M. Trangsrud, A. Tucker, C. Turner, A. Viero, M. Wiebe, D. TI SPIDER OPTIMIZATION: PROBING THE SYSTEMATICS OF A LARGE-SCALE B-MODE EXPERIMENT SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmic microwave background; gravitational waves; methods: data analysis; polarization ID BACKGROUND POLARIZATION MEASUREMENTS; TRANSITION-EDGE SENSORS; 2003 FLIGHT; WMAP OBSERVATIONS; POWER SPECTRUM; CMB TEMPERATURE; ANISOTROPY; BOOMERANG; MULTIPLEXER; INFLATION AB Spider is a long-duration, balloon-borne polarimeter designed to measure large-scale cosmic microwave background (CMB) polarization with very high sensitivity and control of systematics. The instrument will map over half the sky with degree angular resolution in the I, Q, and U Stokes parameters in four frequency bands from 96 to 275 GHz. Spider's ultimate goal is to detect the primordial gravity-wave signal imprinted on the CMB B-mode polarization. One of the challenges in achieving this goal is the minimization of the contamination of B-modes by systematic effects. This paper explores a number of instrument systematics and observing strategies in order to optimize B-mode sensitivity. This is done by injecting realistic-amplitude, time-varying systematics into a set of simulated time streams. Tests of the impact of detector noise characteristics, pointing jitter, payload pendulations, polarization angle offsets, beam systematics, and receiver gain drifts are shown. Spider's default observing strategy is to spin continuously in azimuth, with polarization modulation achieved by either a rapidly spinning half-wave plate or a rapidly spinning gondola and a slowly stepped half-wave plate. Although the latter is more susceptible to systematics, the results shown here indicate that either mode of operation can be used by Spider. C1 [MacTavish, C. J.; Bond, J. R.; Crill, B. P.; Dore, O.] Univ Toronto, CITA, Toronto, ON M5S 3H8, Canada. [Ade, P. A. R.; Tucker, C.] Cardiff Univ, Sch Phys & Astron, Cardiff CF24 3AA, S Glam, Wales. [Battistelli, E. S.; Halpern, M.] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada. [Benton, S.; Netterfield, C. B.; Wiebe, D.] Univ Toronto, Dept Phys, Toronto, ON M5S 3H8, Canada. [Bihary, R.; Bryan, S.; Lawrie, C.; Montroy, T. E.; Riley, D.; Ruhl, J. E.] Case Western Reserve Univ, Dept Phys, Cleveland, OH 44106 USA. [Bock, J. J.; Brevik, J.; Holmes, W.; Jones, W. C.; Turner, A.] Jet Prop Lab, Pasadena, CA 91109 USA. [Bock, J. J.; Golwala, S. R.; Hristov, V. V.; Jones, W. C.; Kuo, C. L.; Lange, A. E.; Mason, P.; Runyan, M.; Trangsrud, A.] CALTECH, Dept Phys, Pasadena, CA 91125 USA. [Contaldi, C. R.] Univ London Imperial Coll Sci Technol & Med, Blackett Lab, London SW7 2A, England. [Crill, B. P.; Fissel, L.; Netterfield, C. B.; Viero, M.] Univ Toronto, Dept Astron & Astrophys, Toronto, ON M5S 3H4, Canada. [Hilton, G.; Irwin, K.] Natl Inst Stand & Technol, Boulder, CO 80305 USA. [Martin, T. G.] Univ Toronto, Dept Mech & Ind Engn, Toronto, ON M5S 3G8, Canada. RP MacTavish, CJ (reprint author), Univ Toronto, CITA, Toronto, ON M5S 3H8, Canada. FU Canada Foundation for Innovation FX This research used the McKenzie cluster at CITA, funded by the Canada Foundation for Innovation. Some of the results in this paper have been derived using the HEALPix package (Gorski et al. 2005), as well as the FFTW package (Frigo & Johnson 2005). We thank the anonymous referee for helpful comments and corrections. NR 49 TC 15 Z9 15 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 DEC 20 PY 2008 VL 689 IS 2 BP 655 EP 665 DI 10.1086/592732 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 376NF UT WOS:000261189600001 ER PT J AU Ajello, M Greiner, J Sato, G Willis, DR Kanbach, G Strong, AW Diehl, R Hasinger, G Gehrels, N Markwardt, CB Tueller, J AF Ajello, M. Greiner, J. Sato, G. Willis, D. R. Kanbach, G. Strong, A. W. Diehl, R. Hasinger, G. Gehrels, N. Markwardt, C. B. Tueller, J. TI COSMIC X-RAY BACKGROUND AND EARTH ALBEDO SPECTRA WITH SWIFT BAT SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmology observations; diffuse radiation; Earth; galaxies: active; X-rays: diffuse background ID ACTIVE GALACTIC NUCLEI; DEEP FIELD-SOUTH; XMM-NEWTON; BLACK-HOLES; GAMMA-RAYS; CHANDRA; AGNS; SPECTROMETERS; POPULATION; TELESCOPE AB We use Swift BAT Earth occultation data at different geomagnetic latitudes to derive a sensitive measurement of the cosmic X-ray background (CXB) and of the Earth albedo emission in the 15-200 keV band. We compare our CXB spectrum with recent (INTEGRAL, BeppoSAX) and past results (HEAO-1) and find good agreement. Using an independent measurement of the CXB spectrum we are able to confirm our results. This study shows that the BAT CXB spectrum has a normalization similar to 8% +/- 3% larger than the HEAO-1 measurement. The BAT accurate Earth albedo spectrum can be used to predict the level of photon background for satellites in low Earth and mid inclination orbits. C1 [Ajello, M.; Greiner, J.; Willis, D. R.; Kanbach, G.; Strong, A. W.; Diehl, R.; Hasinger, G.] Max Planck Inst Extraterr Phys, D-85741 Garching, Germany. [Sato, G.; Gehrels, N.; Markwardt, C. B.; Tueller, J.] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA. RP Ajello, M (reprint author), Max Planck Inst Extraterr Phys, Postfach 1312, D-85741 Garching, Germany. RI Gehrels, Neil/D-2971-2012; Tueller, Jack/D-5334-2012 FU DFG Leibniz-Prize [HA 1850/28-1] FX We are grateful to S. Barthelmy, J. Cummings and H. Krimm for all the effort spent in keeping the BAT perfectly operating. M. A. acknowledges the useful suggestions of R. Mushotzky and the help of C. Gordon for adapting XSPEC to the purposes of this analysis. The anonymous referee is acknowledged for his/her helpful comments which improved the manuscript. M. A. is grateful to S. Sazonov and A. Zoglauer for interesting discussions about the Earth emission. 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. M.A. acknowledges funding from the DFG Leibniz-Prize to G.H. (HA 1850/28-1). NR 44 TC 86 Z9 86 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD DEC 20 PY 2008 VL 689 IS 2 BP 666 EP 677 DI 10.1086/592595 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 376NF UT WOS:000261189600002 ER PT J AU Gehrels, N Barthelmy, SD Burrows, DN Cannizzo, JK Chincarini, G Fenimore, E Kouveliotou, C O'Brien, P Palmer, DM Racusin, J Roming, PWA Sakamoto, T Tueller, J Wijers, RAMJ Zhang, B AF Gehrels, N. Barthelmy, S. D. Burrows, D. N. Cannizzo, J. K. Chincarini, G. Fenimore, E. Kouveliotou, C. O'Brien, P. Palmer, D. M. Racusin, J. Roming, P. W. A. Sakamoto, T. Tueller, J. Wijers, R. A. M. J. Zhang, B. TI CORRELATIONS OF PROMPT AND AFTERGLOW EMISSION IN SWIFT LONG AND SHORT GAMMA-RAY BURSTS SO ASTROPHYSICAL JOURNAL LA English DT Review DE gamma rays: bursts ID SPECTRAL-ENERGY CORRELATIONS; X-RAY; OPTICAL AFTERGLOW; LIGHT CURVES; HOST GALAXY; XRT DATA; MULTIWAVELENGTH AFTERGLOW; COMPREHENSIVE ANALYSIS; CHROMATIC BREAKS; SHALLOW DECAY AB Correlation studies of prompt and afterglow emission from gamma-ray bursts (GRBs) between different spectral bands have been difficult to do in the past because few bursts had comprehensive and comparable afterglow measurements. In this paper we present a large and uniform data set for correlation analysis based on bursts detected by the Swift mission. For the first time, short and long bursts can be analyzed and compared. It is found for both classes that the optical, X-ray, and gamma-ray emission are linearly correlated, but with a large spread about the correlation line; stronger bursts tend to have brighter afterglow, and bursts with brighter X-ray afterglow tend to have brighter optical afterglow. Short bursts are, on average, weaker in both prompt and afterglow emission. No short bursts are seen with extremely low optical Y to YX-ray ratios, as occurs for "dark'' long bursts. Although statistics are still poor for short bursts, there is no evidence yet for a subgroup of short bursts with high extinction, as there is for long bursts. Long bursts are detected in the dark category in the same fraction as pre-Swift bursts. Interesting cases of long bursts that are detected in the optical, and yet have a low enough optical Y to YX-ray ratio to be classified as dark, are discovered. For the prompt emission, short and long bursts have different average tracks on flux versus fluence plots. In Swift, GRB detections tend to be fluence-limited for short bursts and flux-limited for long events. C1 [Gehrels, N.; Barthelmy, S. D.; Cannizzo, J. K.; Sakamoto, T.; Tueller, J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Burrows, D. N.; Racusin, J.; Roming, P. W. A.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Cannizzo, J. K.; Sakamoto, T.] Univ Maryland Baltimore Cty, CRESST, Joint Ctr Astrophys, Baltimore, MD 21250 USA. [Chincarini, G.] INAF Osservatorio Astron Brera, I-23807 Merate, Italy. [Chincarini, G.] Univ Milan, I-20126 Milan, Italy. [Fenimore, E.] Los Alamos Natl Lab, Los Alamos, NM 87545 USA. [Kouveliotou, C.] NSSTC, NASA, Marshall Space Flight Ctr, Huntsville, AL 35805 USA. [O'Brien, P.] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England. [Wijers, R. A. M. J.] Univ Amsterdam, Astron Inst Anton Pannekoek, Fac Sci, NL-1098 SJ Amsterdam, Netherlands. [Zhang, B.] Univ Nevada, Dept Phys & Astron, Las Vegas, NV 89154 USA. RP Gehrels, N (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. EM neil.gehrels@nasa.gov RI Racusin, Judith/D-2935-2012; Barthelmy, Scott/D-2943-2012; Gehrels, Neil/D-2971-2012; Tueller, Jack/D-5334-2012; OI Wijers, Ralph/0000-0002-3101-1808 NR 119 TC 65 Z9 66 U1 0 U2 11 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD DEC 20 PY 2008 VL 689 IS 2 BP 1161 EP 1172 DI 10.1086/592766 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 376NF UT WOS:000261189600038 ER PT J AU Sahai, R Findeisen, K De Paz, AG Contreras, CS AF Sahai, R. Findeisen, K. De Paz, A. Gil Contreras, C. Sanchez TI BINARITY IN COOL ASYMPTOTIC GIANT BRANCH STARS: A GALEX SEARCH FOR ULTRAVIOLET EXCESSES SO ASTROPHYSICAL JOURNAL LA English DT Article DE binaries: general; circumstellar matter; planetary nebulae: general; stars: AGB and post-AGB; stars: mass loss ID HUBBLE-SPACE-TELESCOPE; PLANETARY-NEBULAE; MIRA-B; H-2 EMISSION; V-HYDRAE; OUTFLOW; SPECTRA; DISK; CLASSIFICATION; PERFORMANCE AB The search for binarity in AGB stars is of critical importance for our understanding of how planetary nebulae acquire the dazzling variety of aspherical shapes which characterizes this class. However, detecting binary companions in such stars has been severely hampered due to their extreme luminosities and pulsations. We have carried out a small imaging survey of AGB stars in ultraviolet light (using GALEX), where these cool objects are very faint, in order to search for hotter companions. We report the discovery of significant far-ultraviolet excesses toward nine of these stars. The far-ultraviolet excess most likely results either directly from the presence of a hot binary companion or indirectly from a hot accretion disk around the companion. C1 [Sahai, R.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Findeisen, K.] Cornell Univ, Ithaca, NY 14853 USA. [De Paz, A. Gil] Univ Complutense Madrid, Dept Astrofis, E-28040 Madrid, Spain. [Contreras, C. Sanchez] CSIC, Inst Estructura Mat, Dept Astrofis Mol & Infraroja, E-28006 Madrid, Spain. RP Sahai, R (reprint author), CALTECH, Jet Prop Lab, Mail Stop 183-900, Pasadena, CA 91109 USA. RI Sanchez-Contreras, Carmen/N-3718-2015; Gil de Paz, Armando/J-2874-2016; OI Sanchez-Contreras, Carmen/0000-0002-6341-592X; Gil de Paz, Armando/0000-0001-6150-2854; Findeisen, Krzysztof/0000-0003-1898-5760 FU Spanish Ramon y Cajal program; Programa Nacional de Astronomia y Astrofisica [AYA 2006-02358]; Spanish MCyT [AYA 2006-14876]; Spanish MEC [PIE 200750I028] FX We would like to thank an anonymous referee for his/ her thoughtful review of our paper. We acknowledge discussions with Patrick Morrissey related to the possibility of red leaks in the GALEX FUV and NUV bands. R. S.' s contribution to the research described in this publication was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with NASA. R. S. thanks NASA for financial support via a GALEX award and an LTSA award. K. F. was partially funded by a SURF scholarship and through the Cornell Presidential Research Scholars (CPRS) program. A. G. d. P. is partially financed by the Spanish Ramon y Cajal program and the Programa Nacional de Astronomia y Astrofisica under grant AYA 2006-02358. C. S. C. is partially funded for this work by the Spanish MCyT under project AYA 2006-14876 and the Spanish MEC under project PIE 200750I028. NR 34 TC 21 Z9 21 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD DEC 20 PY 2008 VL 689 IS 2 BP 1274 EP 1278 DI 10.1086/592559 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 376NF UT WOS:000261189600047 ER PT J AU Saumon, D Marley, MS AF Saumon, D. Marley, Mark S. TI THE EVOLUTION OF L AND T DWARFS IN COLOR-MAGNITUDE DIAGRAMS SO ASTROPHYSICAL JOURNAL LA English DT Review DE stars: atmospheres; stars: evolution; stars: low-mass, brown dwarfs ID LOW-MASS STARS; EXTRASOLAR GIANT PLANETS; COLLISION-INDUCED ABSORPTION; BROWN DWARFS; STELLAR ATMOSPHERES; SUBSTELLAR OBJECTS; L/T TRANSITION; INFRARED PHOTOMETRY; THERMAL STRUCTURE; ULTRACOOL DWARFS AB We present new evolution sequences for very low mass stars, brown dwarfs, and giant planets and use them to explore a variety of influences on the evolution of these objects. While the predicted adiabatic evolution of luminosity with time is very similar to results of previous work, the remaining disagreements reveal the magnitude of current uncertainty in brown dwarf evolution theory. We discuss the sources of those differences and argue for the importance of the surface boundary condition provided by atmosphere models including clouds. The L- to T-type ultracool dwarf transition can be accommodated within the Ackerman and Marley cloud model by varying the cloud sedimentation parameter. We develop a simple model for the evolution across the L/T transition. By combining the evolution calculation and our atmosphere models, we generate colors and magnitudes of synthetic populations of ultracool dwarfs in the field and in Galactic clusters. We focus on near-infrared color-magnitude diagrams (CMDs) and on the nature of the "second parameter'' that is responsible for the scatter of colors along the T(eff) sequence. Instead of a single second parameter we find that variations in metallicity and cloud parameters, unresolved binaries, and possibly a relatively young population all play a role in defining the spread of brown dwarfs along the cooling sequence. We also find that the transition from cloudy L dwarfs to cloudless T dwarfs slows down the evolution and causes a pileup of substellar objects in the transition region, in contradiction with previous studies. However, the same model is applied to the Pleiades brown dwarf sequence with less success. Taken at face value, the present Pleiades data suggest that the L/T transition occurs at lower T(eff) for lower gravity objects, such as those found in young Galactic clusters. The simulated populations of brown dwarfs also reveal that the phase of deuterium burning produces a distinctive feature in CMDs that should be detectable in similar to 50-100 Myr old clusters. C1 [Saumon, D.] Los Alamos Natl Lab, Los Alamos, NM 87545 USA. [Marley, Mark S.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Saumon, D (reprint author), Los Alamos Natl Lab, POB 1663,Mail Stop F663, Los Alamos, NM 87545 USA. EM dsaumon@lanl.gov; mark.s.marley@nasa.gov RI Marley, Mark/I-4704-2013 NR 105 TC 218 Z9 218 U1 1 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD DEC 20 PY 2008 VL 689 IS 2 BP 1327 EP 1344 DI 10.1086/592734 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 376NF UT WOS:000261189600051 ER PT J AU Rowe, JF Matthews, JM Seager, S Miller-Ricci, E Sasselov, D Kuschnig, R Guenther, DB Moffat, AFJ Rucinski, SM Walker, GAH Weiss, WW AF Rowe, Jason F. Matthews, Jaymie M. Seager, Sara Miller-Ricci, Eliza Sasselov, Dimitar Kuschnig, Rainer Guenther, David B. Moffat, Anthony F. J. Rucinski, Slavek M. Walker, Gordon A. H. Weiss, Werner W. TI THE VERY LOW ALBEDO OF AN EXTRASOLAR PLANET: MOST(1) SPACE-BASED PHOTOMETRY OF HD 209458 SO ASTROPHYSICAL JOURNAL LA English DT Article DE planetary systems; stars: individual (HD 209458); techniques: photometric ID GIANT PLANETS; THERMAL EMISSION; HOT JUPITERS; ATMOSPHERES; MODELS; SATELLITE; INVERSION; HD-209458; SPECTRUM; SEARCH AB Measuring the albedo of an extrasolar planet provides insight into its atmospheric composition and its global thermal properties, including heat dissipation and weather patterns. Such a measurement requires very precise photometry of a transiting system, fully sampling many phases of the secondary eclipse. Space-based optical photometry of the transiting system HD 209458 from the MOST (Microvariablity and Oscillations of Stars) satellite, spanning 14 and 44 days in 2004 and 2005, respectively, allows us to set a sensitive limit on the optical eclipse of the hot exosolar giant planet in this system. Our best fit to the observations yields a flux ratio of the planet and star of 7 +/- 9 ppm ( parts per million), which corresponds to a geometric albedo through the MOST bandpass (400-700 nm) of A(g) = 0.038 +/- 0.045. This gives a 1 sigma upper limit of 0.08 for the geometric albedo and a 3 sigma upper limit of 0.17. HD 209458b is significantly less reflective than Jupiter ( for which A(g)would be about 0.5). This low geometric albedo rules out the presence of bright reflective clouds in this exoplanet's atmosphere. We determine refined parameters for the star and exoplanet in the HD 209458 system based on a model fit to the MOST light curve. C1 [Rowe, Jason F.] NASA, Moffett Field, CA 94035 USA. [Seager, Sara] MIT, Cambridge, MA 02159 USA. [Miller-Ricci, Eliza; Sasselov, Dimitar] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Kuschnig, Rainer; Walker, Gordon A. H.] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada. [Guenther, David B.] St Marys Univ, Dept Phys & Astron, Halifax, NS B3H 3C3, Canada. [Moffat, Anthony F. J.] Univ Montreal, Dept Phys, Montreal, PQ H3C 3J7, Canada. [Rucinski, Slavek M.] Univ Toronto, David Dunlap Observ, Richmond Hill, ON L4C 4Y6, Canada. [Weiss, Werner W.] Univ Vienna, Inst Astron, A-1180 Vienna, Austria. RP Rowe, JF (reprint author), NASA, Ames Res Pk,Mail Stop 244-30, Moffett Field, CA 94035 USA. EM jasonfrowe@gmail.com FU Natural Sciences and Engineering Research Council (NSERC) Canada; Canadian Space Agency; Austrian Science Promotion Agency (FFG-MOST); Austrian Science Fonds [FWF-P17580] FX The contributions of J.M.M., D. B. G., A. F. J. M., S. M. R., and G. A. H. W. are supported by funding from the Natural Sciences and Engineering Research Council (NSERC) Canada. R. K. is funded by the Canadian Space Agency. W. W. W. received financial support from the Austrian Science Promotion Agency (FFG-MOST) and the Austrian Science Fonds (FWF-P17580). NR 33 TC 114 Z9 115 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD DEC 20 PY 2008 VL 689 IS 2 BP 1345 EP 1353 DI 10.1086/591835 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 376NF UT WOS:000261189600052 ER PT J AU Hartlep, T Zhao, JW Mansour, NN Kosovichev, AG AF Hartlep, Thomas Zhao, Junwei Mansour, Nagi N. Kosovichev, Alexander G. TI VALIDATING TIME-DISTANCE FAR-SIDE IMAGING OF SOLAR ACTIVE REGIONS THROUGH NUMERICAL SIMULATIONS SO ASTROPHYSICAL JOURNAL LA English DT Article DE methods: numerical; Sun: helioseismology; Sun: oscillations; sunspots ID SUN; HELIOSEISMOLOGY; INVERSION; OSCILLATIONS; SUNSPOTS AB Far-side imaging using time-distance helioseismology methods is assessed using numerically generated artificial data. The data are generated using direct numerical simulations of acoustic oscillations in a spherical solar model. Localized variations of the sound speed in the surface and subsurface layers are used to model the perturbations associated with sunspots and active regions. The accuracy of acoustic travel-time far-side maps is shown to depend on the size and location of active regions. Potential artifacts in the far-side imaging procedure, such as those caused by the presence of active regions on the solar near side, are also investigated. C1 [Hartlep, Thomas; Mansour, Nagi N.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Zhao, Junwei; Kosovichev, Alexander G.] Stanford Univ, WW Hansen Expt Phys Lab, Stanford, CA 94305 USA. RP Hartlep, T (reprint author), NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RI Zhao, Junwei/A-1177-2007; OI Hartlep, Thomas/0000-0002-5062-9507 FU NASA's; NASA Postdoctoral Program; Oak Ridge Associated Universities; NASA's "Columbia''; NASA Science Mission Directorate (SMD) High-End Computing (HEC) FX This work was supported by NASA's "Living With a Star'' program. Support from the NASA Postdoctoral Program administered by Oak Ridge Associated Universities is gratefully acknowledged. Simulations were performed on NASA's "Columbia'' supercomputer system. Support by NASA Science Mission Directorate (SMD) High-End Computing (HEC) is gratefully acknowledged. NR 29 TC 13 Z9 13 U1 1 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 DEC 20 PY 2008 VL 689 IS 2 BP 1373 EP 1378 DI 10.1086/592721 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 376NF UT WOS:000261189600054 ER PT J AU Falconer, DA Moore, RL Gary, GA AF Falconer, D. A. Moore, R. L. Gary, G. A. TI MAGNETOGRAM MEASURES OF TOTAL NONPOTENTIALITY FOR PREDICTION OF SOLAR CORONAL MASS EJECTIONS FROM ACTIVE REGIONS OF ANY DEGREE OF MAGNETIC COMPLEXITY SO ASTROPHYSICAL JOURNAL LA English DT Article DE Sun: coronal mass ejections (CMEs); Sun: magnetic fields ID FLARES AB For investigating the magnetic causes of coronal mass ejections (CMEs) and for forecasting the CME productivity of active regions, in previous work we have gauged the total nonpotentiality of a whole active region by either of two measures, L(SSM) and L(SGM), two measures of the magnetic field along the main neutral line in a vector magnetogram of the active region. This previous work was therefore restricted to nominally bipolar active regions, active regions that have a clearly identifiable main neutral line. In the present paper, we show that our work can be extended to include multipolar active regions of any degree of magnetic complexity by replacing L(SSM) and L(SGM) with their generalized counterparts, WL(SS) and WL(SG), which are corresponding integral measures covering all neutral lines in an active region instead of only the main neutral line. In addition, we show that for active regions within 30 heliocentric degrees of disk center, WL(SG) can be adequately measured from line-of-sight magnetograms instead of vector magnetograms. This approximate measure of active-region total nonpotentiality, (L)WL(SG), with the extensive set of 96 minute cadence full-disk line-of-sight magnetograms from SOHO MDI, can be used to study the evolution of active-region total nonpotentiality leading to the production of CMEs. C1 [Falconer, D. A.; Moore, R. L.; Gary, G. A.] NASA, George C Marshall Space Flight Ctr, Dept Space Sci, Huntsville, AL 35812 USA. RP Falconer, DA (reprint author), Univ Alabama, Dept Phys, Huntsville, AL 35899 USA. EM david.a.falconer@nasa.gov; ron.moore@nasa.gov; allen.gary@nasa.gov FU NSF's Division of Atmospheric Sciences through its SHINE and Space Weather; NASA's Science Mission Directorate through the Living With a Star Targeted Research and Technology FX This work was supported by funding from NSF's Division of Atmospheric Sciences through its SHINE and Space Weather programs, and by NASA's Science Mission Directorate through the Living With a Star Targeted Research and Technology program of its Heliophysics Division. We acknowledge the use of the SOHO LASCO CME Catalog generated and maintained by the Center of Solar Physics and Space Weather of the Catholic University of America in cooperation with the Naval Research Laboratory and NASA. SOHO is a project of international cooperation between ESA and NASA. NR 26 TC 26 Z9 26 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD DEC 20 PY 2008 VL 689 IS 2 BP 1433 EP 1442 DI 10.1086/591045 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 376NF UT WOS:000261189600060 ER PT J AU Rodgers, SD Charnley, SB AF Rodgers, S. D. Charnley, S. B. TI NITROGEN ISOTOPIC FRACTIONATION OF INTERSTELLAR NITRILES SO ASTROPHYSICAL JOURNAL LA English DT Article DE astrochemistry; comets: general; ISM: molecules; meteors, meteoroids; molecular processes ID GAS-PHASE REACTIONS; BOPP C/1995 O1; MOLECULAR CLOUDS; PRESTELLAR CORES; GRAIN PROCESSES; UMIST DATABASE; ORGANIC-MATTER; STAR-FORMATION; SOLID-PHASE; SOLAR-WIND AB In light of recent measurement of nitrogen isotope ratios in CN and HCN in several comets, and the correlation between (15)N excess and the presence of nitrile (-CN) functional groups in meteoritic samples, we have reassessed the potential of interstellar chemistry to directly fractionate nitriles. We focus in particular on the (15)N chemistry in selective depletion cores where O-bearing molecules are depleted yet N- and C-bearing species remain in the gas, as revealed by the recent detection of CN in dense CO-depleted cores. We show that large HC(15)N/HC(14)N ratios can be generated if the reaction of CN with N has a barrier, and suggest that cometary HCN and CN may trace material originally formed in dense interstellar clouds. C1 [Rodgers, S. D.; Charnley, S. B.] NASA, Ames Res Ctr, Space Sci & Astrobiol Div, Moffett Field, CA 94035 USA. RP Rodgers, SD (reprint author), NASA, Ames Res Ctr, Space Sci & Astrobiol Div, MS 245-3, Moffett Field, CA 94035 USA. EM rodgers@dusty.arc.nasa.gov RI Charnley, Steven/C-9538-2012 FU NASA's Origins of Solar Systems Program through NASA Ames Cooperative [NNX07AO86A]; SETI Institute FX This work was supported by NASA's Origins of Solar Systems Program through NASA Ames Cooperative agreement NNX07AO86A with the SETI Institute. NR 70 TC 32 Z9 32 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD DEC 20 PY 2008 VL 689 IS 2 BP 1448 EP 1455 DI 10.1086/592195 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 376NF UT WOS:000261189600062 ER PT J AU Hailey-Dunsheath, S Nikola, T Stacey, GJ Oberst, TE Parshley, SC Bradford, CM Ade, PAR Tucker, CE AF Hailey-Dunsheath, S. Nikola, T. Stacey, G. J. Oberst, T. E. Parshley, S. C. Bradford, C. M. Ade, P. A. R. Tucker, C. E. TI DETECTION OF THE (CO)-C-13 J=6 -> 5 TRANSITION IN THE STARBURST GALAXY NGC 253 SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE galaxies: individual (NGC 253); galaxies: ISM; galaxies: nuclei; galaxies: starburst; ISM: molecules; submillimeter ID WARM MOLECULAR GAS; INTER-STELLAR CLOUDS; DENSE GAS; CIRCUMNUCLEAR DISK; INFRARED-EMISSION; NUCLEAR STARBURST; THERMAL BALANCE; NEARBY GALAXIES; CARBON-MONOXIDE; VELOCITY-FIELD AB We report the detection of (CO)-C-13 J = 6 -> 5 emission from the nucleus of the starburst galaxy NGC 253 with the redshift (z) and Early Universe Spectrometer (ZEUS), a new submillimeter grating spectrometer. This is the first extragalactic detection of the (CO)-C-13 J = 6 -> 5 transition, which traces warm, dense molecular gas. We employ a multiline LVG analysis and find approximate to 35%-60% of the molecular interstellar medium is both warm (T similar to 110 K) and dense (n(H2) similar to 10(4) cm(-3)). We analyze the potential heat sources and conclude that ultraviolet and X-ray photons are unlikely to be energetically important. Instead, the molecular gas is most likely heated by an elevated density of cosmic rays or by the decay of supersonic turbulence through shocks. If the cosmic rays and turbulence are created by stellar feedback within the starburst, then our analysis suggests the starburst may be self-limiting. C1 [Hailey-Dunsheath, S.; Nikola, T.; Stacey, G. J.; Oberst, T. E.; Parshley, S. C.] Cornell Univ, Dept Astron, Ithaca, NY 14853 USA. [Bradford, C. M.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Ade, P. A. R.; Tucker, C. E.] Cardiff Univ, Dept Phys & Astron, Cardiff CF24 3AA, S Glam, Wales. RP Hailey-Dunsheath, S (reprint author), Cornell Univ, Dept Astron, Ithaca, NY 14853 USA. EM steve@astro.cornell.edu FU NSF [AST 00-96881, AST 03-52855, AST 07-05256, AST 07-22220]; NASA [NGT 05-50470, NNG 05-GK70H] FX This work was supported by NSF grants AST 00-96881, AST 03-52855, AST 07-05256, and AST 07-22220, and by NASA grants NGT 05-50470 and NNG 05-GK70H. We are indebted to the GSFC group (C. A. Allen, S. H. Moseley, D. J. Benford, and J. G. Staguhn) for their sensitive bolometers. We also thank the CSO staff for their support of ZEUS operations and an anonymous referee for many helpful comments on an earlier draft of this manuscript. NR 38 TC 31 Z9 31 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD DEC 20 PY 2008 VL 689 IS 2 BP L109 EP L112 DI 10.1086/595840 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 398LQ UT WOS:000262734000008 ER PT J AU Krennrich, F Dwek, E Imran, A AF Krennrich, F. Dwek, E. Imran, A. TI CONSTRAINTS ON ENERGY SPECTRA OF BLAZARS BASED ON RECENT EBL LIMITS FROM GALAXY COUNTS SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE BL Lacertae objects: individual (1ES 1218+30.4, 1ES 1101-232; 1ES 0229+200) ID EXTRAGALACTIC BACKGROUND LIGHT; SPITZER-SPACE-TELESCOPE; VHE GAMMA-RAYS; TEV BLAZARS; MU-M; DISCOVERY; RADIATION; ACCELERATION; EVOLUTION; EMISSION AB We combine the recent estimate of the contribution of galaxies to the 3.6 mu m intensity of the extragalactic background light (EBL) with optical and near-infrared (IR) galaxy counts to set new limits on intrinsic spectra of some of the most distant TeV blazars, 1ES 0229+200, 1ES 1218+30.4, and 1ES 1101-232, located at redshifts 0.1396, 0.182, and 0.186, respectively. The new lower limit on the 3.6 mm EBL intensity is significantly higher than the previous one set by the cumulative emission from resolved Spitzer galaxies. Correcting for attenuation by the revised EBL, we show that the differential spectral index of the intrinsic spectrum of the three blazars is or harder. These results present blazar emission models with the challenge of producing 1.28 +/- 0.20 extremely hard intrinsic spectra in the sub-TeV to multi-TeV regime. These results also question the reliability of recently derived upper limits on the near-IR EBL intensity that are solely based on the assumption that intrinsic blazar spectra should not be harder than 1.50. C1 [Krennrich, F.; Imran, A.] Iowa State Univ, Dept Phys & Astron, Ames, IA 50011 USA. [Dwek, E.] NASA, Goddard Space Flight Ctr, Observat Cosmol Lab, Greenbelt, MD 20771 USA. RP Krennrich, F (reprint author), Iowa State Univ, Dept Phys & Astron, Ames, IA 50011 USA. EM krennrich@iastate.edu; eli.dwek@nasa.gov RI Dwek, Eli/C-3995-2012 FU US Department of Energy; NASA [LTSA 03-0000-065] FX This research is supported by grants from the US Department of Energy. The authors thank W. Benbow and W. Hofmann for providing the spectral data for 1ES 1101-232 and 1ES 0229+200. We also thank P. Fortin and the VERITAS collaboration for providing the 1ES 1218+30.4 data. E. D. acknowledges the support of NASA LTSA 03-0000-065. NR 33 TC 19 Z9 19 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD DEC 20 PY 2008 VL 689 IS 2 BP L93 EP L96 DI 10.1086/595960 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 398LQ UT WOS:000262734000004 ER PT J AU Campbell, B Carter, L Phillips, R Plaut, J Putzig, N Safaeinili, A Seu, R Biccari, D Egan, A Orosei, R AF Campbell, Bruce Carter, Lynn Phillips, Roger Plaut, Jeffrey Putzig, Nathaniel Safaeinili, Ali Seu, Roberto Biccari, Daniela Egan, Anthony Orosei, Roberto TI SHARAD radar sounding of the Vastitas Borealis Formation in Amazonis Planitia SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Article ID ORBITER LASER ALTIMETER; NORTHERN LOWLANDS; FLOOD LAVAS; MOLA DATA; MARS; VOLCANISM; DEPOSITS; PLAINS; FATE AB Amazonis Planitia has undergone alternating episodes of sedimentary and volcanic infilling, forming an interleaved sequence with an upper surface that is very smooth at the kilometer scale. Earlier work interprets the near-surface materials as either young, rough lava flows or ice-rich sediment layers, overlying a basement comprising the Vastitas Borealis Formation and earlier Hesperian plains. Sounding radar profiles across Amazonis Planitia from the Shallow Radar (SHARAD) instrument on the Mars Reconnaissance Orbiter reveal a subsurface dielectric interface that increases in depth toward the north along most orbital tracks. The maximum depth of detection is 100-170 m, depending upon the real dielectric permittivity of the materials, but the interface may persist at greater depth to the north if the reflected energy is attenuated below the SHARAD noise floor. The dielectric horizon likely marks the boundary between sedimentary material of the Vastitas Borealis Formation and underlying Hesperian volcanic plains. The SHARAD-detected interface follows the surface topography across at least one of the large wrinkle ridges in north central Amazonis Planitia. This conformality suggests that Vastitas Borealis sediments, at least in this region, were emplaced prior to compressional tectonic deformation. The change in radar echo strength with time delay is consistent with a loss tangent of 0.005-0.012 for the column of material between the surface and the reflector. These values are consistent with dry, moderate-density sediments or the lower end of the range of values measured for basalts. While a component of distributed ice in a higher-loss matrix cannot be ruled out, we do not find evidence for a dielectric horizon within the Vastitas Borealis Formation that might suggest an abrupt change from an upper dry layer to an ice-rich lower deposit. C1 [Campbell, Bruce; Carter, Lynn] Smithsonian Inst, Ctr Earth & Planetary Studies, Washington, DC 20013 USA. [Seu, Roberto; Biccari, Daniela] Univ Roma La Sapienza, INFOCOM, I-00184 Rome, Italy. [Phillips, Roger; Putzig, Nathaniel; Egan, Anthony] SW Res Inst, Boulder, CO 80302 USA. [Orosei, Roberto] Ist Astrofis Spaziale & Fis Cosm, I-00133 Rome, Italy. [Plaut, Jeffrey; Safaeinili, Ali] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Campbell, B (reprint author), Smithsonian Inst, Ctr Earth & Planetary Studies, MRC 315,POB 37012, Washington, DC 20013 USA. EM campbellb@si.edu RI Carter, Lynn/D-2937-2012 NR 26 TC 18 Z9 18 U1 0 U2 2 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 DEC 20 PY 2008 VL 113 IS E12 AR E12010 DI 10.1029/2008JE003177 PG 10 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 386MI UT WOS:000261886900002 ER PT J AU Yingst, RA Crumpler, L Farrand, WH Li, R Cabrol, NA Neakrase, LD AF Yingst, R. A. Crumpler, L. Farrand, W. H. Li, R. Cabrol, N. A. Neakrase, L. D. TI Morphology and texture of particles along the Spirit rover traverse from sol 450 to sol 745 SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Article ID PATHFINDER LANDING SITE; GUSEV CRATER; ROCK PARTICLES; MARS; SHAPE; ROUNDNESS; SIZE; DISTRIBUTIONS; INDICATORS; PLANETARY AB We quantified and classified the shape, roundness, size, and texture of 935 loose surface particles along the Spirit rover traverse from sols 450-745 to assess origin, transport, and other alteration mechanisms that altered particles during and after formation. Variation in particle morphologic parameters along traverse is consistent with crossing mapped geologic unit boundaries. Texture is divided into four types: vesicular, smooth and flat-faceted, rough and flat-faceted, and very rough. Sphericity and roundness are intermediate and low, respectively, comparable to particles moved by high-energy transport or to crushed particles. This indicates intermittent, high-energy emplacement or modification of a single lithology, rather than systematic, continuous low-energy abrasion or wear over time. Comparison with particle morphology at other Mars landing sites is consistent with the hypothesis that no secondary systematic transport or wide-scale chemical alteration was active at a significant enough level to alter macromorphology. In particular, particle morphology at the Mars Pathfinder site shows stronger evidence of abrasion than along the Spirit traverse, suggesting Mars Pathfinder particles have undergone abrasion processes that particles in this study area have not. Additionally, morphology indices have correlation coefficients near zero, indicating that a fluvial transport mechanism is likely not responsible for morphology. Morphology and texture are instead related to origin and composition rather than subsequent modification. Morphology and texture support a volcanic origin, possibly without modification, but most likely altered primarily by ballistic impact, implying that the Spirit landing site and traverse may be utilized in the future as a standard site for characterization of impact-derived morphology. C1 [Yingst, R. A.] Univ Wisconsin Green Bay, Dept Nat & Appl Sci, Green Bay, WI 54311 USA. [Cabrol, N. A.] NASA, Ames Res Ctr, Div Space Sci, Moffett Field, CA 94035 USA. [Crumpler, L.] New Mexico Museum Nat Hist & Sci, Albuquerque, NM 87104 USA. [Farrand, W. H.] Space Sci Inst, Boulder, CO 80301 USA. [Li, R.] Ohio State Univ, Dept Civil Engn, Columbus, OH 43210 USA. [Neakrase, L. D.] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85287 USA. RP Yingst, RA (reprint author), Univ Wisconsin Green Bay, Dept Nat & Appl Sci, 2420 Nicolet Dr, Green Bay, WI 54311 USA. EM yingsta@uwgb.edu FU Mars Exploration Rover Program through JPL [1278721] FX We gratefully acknowledge the constructive reviews of J. Zimbelman and B. Ehlmann, whose comments greatly improved this manuscript. Undergraduates Cassandra Marnocha and Zachary Christman collected portions of the data. This research was supported by the Mars Exploration Rover Program through JPL contract 1278721 to R.A.Y. NR 73 TC 16 Z9 16 U1 0 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 DEC 20 PY 2008 VL 113 IS E12 AR E12S41 DI 10.1029/2008JE003179 PG 17 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 386MI UT WOS:000261886900003 ER PT J AU Miyashita, Y Hosokawa, K Hori, T Kamide, Y Yukimatu, AS Fujimoto, M Mukai, T Machida, S Sato, N Saito, Y Shinohara, I Sigwarth, JB AF Miyashita, Y. Hosokawa, K. Hori, T. Kamide, Y. Yukimatu, A. S. Fujimoto, M. Mukai, T. Machida, S. Sato, N. Saito, Y. Shinohara, I. Sigwarth, J. B. TI Response of large-scale ionospheric convection to substorm expansion onsets: A case study SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article ID HIGH-LATITUDE CONVECTION; EARTHWARD FLOW BURSTS; SHEET BOUNDARY-LAYER; AURORAL RADAR NETWORK; THIN CURRENT SHEETS; PLASMA SHEET; MAGNETOSPHERIC SUBSTORMS; MIDDISTANT MAGNETOTAIL; GEOTAIL OBSERVATIONS; CURRENT SIGNATURES AB We have studied the response of large-scale ionospheric convection to substorm expansion onsets on the basis of two weak substorms of 1 May 2001, during which a large part of the dawn cell of the two-cell ionospheric convection pattern was monitored by the SuperDARN radars. Ionospheric convection began to enhance first in a localized region of the equatorward part of the dawn cell similar to 2 minutes before the expansion onsets of both substorms and then enhanced in the entire dawn cell successively. The enhanced convection persisted throughout their expansion phase, possibly even near the footprint of a plasma sheet region without fast flows observed by Geotail. These observations suggest that ionospheric convection begins to enhance just before substorm expansion onset and then enhances in the entire cell, possibly regardless of the presence of fast earthward flows in the corresponding plasma sheet region of the magnetotail. The global enhancement of ionospheric convection is consistent with that of magnetotail convection, which also begins just before onset. C1 [Miyashita, Y.; Fujimoto, M.; Mukai, T.; Saito, Y.; Shinohara, I.] Japan Aerosp Explorat Agcy, Inst Space & Astronaut Sci, Sagamihara, Kanagawa 2298510, Japan. [Hosokawa, K.] Univ Electrocommun, Dept Informat & Commun Engn, Tokyo 1828585, Japan. [Hori, T.] Nagoya Univ, Solar Terr Environm Lab, Chikusa Ku, Nagoya, Aichi 4648601, Japan. [Kamide, Y.] Kyoto Univ, Res Inst Sustainable Humanosphere, Kyoto 6110011, Japan. [Yukimatu, A. S.; Sato, N.] Natl Inst Polar Res, Itabashi Ku, Tokyo 1738515, Japan. [Machida, S.] Kyoto Univ, Dept Geophys, Sakyo Ku, Kyoto 6068502, Japan. [Sigwarth, J. B.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Miyashita, Y (reprint author), Japan Aerosp Explorat Agcy, Inst Space & Astronaut Sci, 3-1-1 Yoshinodai, Sagamihara, Kanagawa 2298510, Japan. EM miyasita@stp.isas.jaxa.jp OI Hori, Tomoaki/0000-0001-8451-6941 FU University of Iowa; National Aeronautics and Space Administration [NAG5-11528] FX We thank S. Kokubun and T. Nagai for providing the Geotail MGF magnetic field data. We also thank R. W. McEntire, S. P. Christon, and A. T. Y. Lui for the Geotail EPIC-STICS high-energy particle data and M. Nose, D. Nagata, and Y. Ono for preparing them. The ACE SWEPAM plasma data, the ACE MAG magnetic field data, and the GOES magnetic field data were provided by D. J. McComas, N. Ness, and H. J. Singer, respectively, through the Coordinated Data Analysis Web (CDAWeb) at NASA. The CANOPUS MSP auroral data were provided by F. Creutzberg and E. Donovan, and the CANOPUS and CANMOS geomagnetic field data were provided by I. Mann and D. Boteler, respectively, through the Canadian Space Science Data Portal (CSSDP). The Sym-H and Dst indices were provided by World Data Center for Geomagnetism, Kyoto. The Polar UVI auroral imager data were provided by K. Liou and G. K. Parks. The IMAGE FUV auroral imager data were provided by S. B. Mende. We thank all the staff who contributed to the operation of the SuperDARN radars. We also thank F. Creutzberg for his useful comments. This research was supported in part at the University of Iowa by the National Aeronautics and Space Administration under NAG5-11528. NR 63 TC 12 Z9 12 U1 0 U2 2 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0148-0227 J9 J GEOPHYS RES-SPACE JI J. Geophys. Res-Space Phys. PD DEC 20 PY 2008 VL 113 IS A12 AR A12309 DI 10.1029/2008JA013586 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 386MT UT WOS:000261888000001 ER PT J AU Singh, M Asthana, R Shpargel, TP AF Singh, M. Asthana, R. Shpargel, T. P. TI Brazing of ceramic-matrix composites to Ti and Hastealloy using Ni-base metallic glass interlayers SO MATERIALS SCIENCE AND ENGINEERING A-STRUCTURAL MATERIALS PROPERTIES MICROSTRUCTURE AND PROCESSING LA English DT Article; Proceedings Paper CT 2nd International Conference on Recent Advances in Composite Materials CY FEB 20-23, 2007 CL New Delhi, INDIA SP India Habitat Ctr DE Metallic glass; Brazing; C-C composite; C-SiC composite; SiC-SiC composite; Scanning electron microscopy; Energy dispersive spectroscopy; Knoop microhardness ID CARBON-CARBON COMPOSITES; TITANIUM AB Carbon-carbon, carbon-silicon carbide, and silicon carbide-silicon carbide composites were vacuum brazed to Ti and Hastealloy X using Ni-base metallic glass braze foils (MBF-20 and MBF-30). Scanning electron microscopy (SEM) and energy-dispersive X-ray spectroscopy (EDS) of the joints showed that compositional changes due to substrate dissolution led to secondary-phase precipitation which aided interfacial bonding although inter-laminar shear failure occurred within some composites. Residual thermal stresses in the joint led to hardness gradients; however, stress accommodation by the brazes prevented interfacial cracking. The peak Knoop microhardness in the joints was as high as 1165-1294 KHN. (C) 2008 Elsevier B.V. All rights reserved. C1 [Singh, M.] NASA, Glenn Res Ctr, Ohio Aerosp Inst, ASRC Aerosp, Cleveland, OH 44135 USA. [Asthana, R.] Univ Wisconsin Stout, Dept Engn & Technol, Menomonie, WI 54751 USA. RP Singh, M (reprint author), NASA, Glenn Res Ctr, Ohio Aerosp Inst, ASRC Aerosp, Cleveland, OH 44135 USA. EM Mrityunjay.Singh-1@grc.nasa.gov NR 22 TC 56 Z9 66 U1 3 U2 17 PU ELSEVIER SCIENCE SA PI LAUSANNE PA PO BOX 564, 1001 LAUSANNE, SWITZERLAND SN 0921-5093 J9 MAT SCI ENG A-STRUCT JI Mater. Sci. Eng. A-Struct. Mater. Prop. Microstruct. Process. PD DEC 20 PY 2008 VL 498 IS 1-2 SI SI BP 19 EP 30 DI 10.1016/j.msea.2007.11.150 PG 12 WC Nanoscience & Nanotechnology; Materials Science, Multidisciplinary; Metallurgy & Metallurgical Engineering SC Science & Technology - Other Topics; Materials Science; Metallurgy & Metallurgical Engineering GA 379UA UT WOS:000261420500005 ER PT J AU Singh, M Morscher, GN Shpargel, TP Asthana, R AF Singh, M. Morscher, Gregory N. Shpargel, Tarah P. Asthana, Rajiv TI Active metal brazing of titanium to high-conductivity carbon-based sandwich structures SO MATERIALS SCIENCE AND ENGINEERING A-STRUCTURAL MATERIALS PROPERTIES MICROSTRUCTURE AND PROCESSING LA English DT Article; Proceedings Paper CT 2nd International Conference on Recent Advances in Composite Materials CY FEB 20-23, 2007 CL New Delhi, INDIA SP India Habitat Ctr DE Brazing; Carbon foam; C-C composite; Shear stress; Knoop microhardness; Scanning electron microscopy; Energy-dispersive spectroscopy AB Reactive brazing technology was developed and processing parameters were optimized for the bonding of titanium tubes, graphite foam, and high-conductivity carbon-carbon composite face sheets using the active braze Cusil-ABA paste and foils. The microstructure and composition of the joints, examined using scanning electron microscopy coupled with energy-dispersive spectroscopy, showed good bonding and braze penetration in all systems when braze paste was used. The hardness values of the brazed joints were consistent for the different specimen stacking configurations. Mechanical testing of Ti tube/foam/C-C composite structures both in tension and shear showed that failure always occurred in the foam material demonstrating that the brazed joint was sufficient for these types of sandwich structures. (C) 2008 Elsevier B.V. All rights reserved. C1 [Singh, M.; Morscher, Gregory N.] NASA, Glenn Res Ctr, Ohio Aerosp Inst, ASRC Aerosp, Cleveland, OH 44135 USA. [Asthana, Rajiv] Univ Wisconsin Stout, Dept Engn & Technol, Menomonie, WI 54751 USA. RP Singh, M (reprint author), NASA, Glenn Res Ctr, Ohio Aerosp Inst, ASRC Aerosp, MS 106-5, Cleveland, OH 44135 USA. EM Mrityunjay.Singh@grc.nasa.gov NR 5 TC 22 Z9 23 U1 2 U2 9 PU ELSEVIER SCIENCE SA PI LAUSANNE PA PO BOX 564, 1001 LAUSANNE, SWITZERLAND SN 0921-5093 J9 MAT SCI ENG A-STRUCT JI Mater. Sci. Eng. A-Struct. Mater. Prop. Microstruct. Process. PD DEC 20 PY 2008 VL 498 IS 1-2 SI SI BP 31 EP 36 DI 10.1016/j.msea.2007.11.151 PG 6 WC Nanoscience & Nanotechnology; Materials Science, Multidisciplinary; Metallurgy & Metallurgical Engineering SC Science & Technology - Other Topics; Materials Science; Metallurgy & Metallurgical Engineering GA 379UA UT WOS:000261420500006 ER PT J AU Kalashnikova, OV Kahn, RA AF Kalashnikova, Olga V. Kahn, Ralph A. TI Mineral dust plume evolution over the Atlantic from MISR and MODIS aerosol retrievalsy SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID REMOTE-SENSING OBSERVATIONS; OPTICAL DEPTH; SAHARAN DUST; INTERANNUAL VARIABILITY; FORECAST MODEL; ART.; SENSITIVITY; AERONET; SIMULATIONS; ASSESSMENTS AB We demonstrate how Multiangle Imaging Spectroradiometer ( MISR) and Moderate Resolution Imaging Spectroradiometer ( MODIS) space-based aerosol products provide complementary information, characterizing ( 1) transported desert dust plume extent over water, ( 2) aerosol optical thickness ( AOT) evolution, and ( 3) particle size sensitivity and fraction spherical evolution for the thicker parts of these plumes. MODIS provides more extensive coverage, whereas MISR's multiangle retrievals include dust properties and fill in areas where glint precludes MODIS optical depth retrievals, increasing by up to 50% dust plume surface area coverage compared to MODIS-only observations. These results can be used to improve dust aerosol representations in climate, forecast, and transport models. Extensive comparison of MISR and MODIS AOT retrievals with Aerosol Robotic Network ( AERONET) observations in dusty regions show accuracies of about 20%; MISR Angstrom exponent is predominantly less than 1, in reasonably good agreement with AERONET. For four selected North African dust transport events, combined MISR and MODIS observations map systematic changes in retrieved plume surface area, on the basis of AOT contours; these reflect differences in aerosol dispersion and removal rates that must be reproduced by models. Within MISR retrieval uncertainties, Angstrom exponent and AOT fraction spherical are lower in the optically thicker parts of the plume by up to 30% and increase as the plume is transported across the ocean, as would be expected; retrieved single-scattering albedo values are similar to 0.98 for all stages of plume evolution. For the cases studied, AERONET shows similar property patterns at points on either side of the Atlantic and indicates similar to 15% decrease in aerosol coarse mode effective radius during transoceanic transport. C1 [Kalashnikova, Olga V.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Kahn, Ralph A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Kalashnikova, OV (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM olga.v.kalashnikova@jpl.nasa.gov RI Kahn, Ralph/D-5371-2012 OI Kahn, Ralph/0000-0002-5234-6359 FU NASA Earth Sciences Division FX We thank Michael Garay for creating tools for collocating MISR and MODIS aerosol retrievals; Amy Braverman, PI of AMAPS project, for her help in developing tools for obtaining and comparing MISR, MODIS, and AERONET data; and the AERONET project and the Saharan AERONET stations principal investigators for their efforts in establishing and maintaining the nine sites used in this investigation. We thank Jeffrey Reid and Douglas Westphal for sharing NAAPS data and the MISR team for providing facilities, access to data, and useful discussions. The work of O. Kalashnikova is supported by a grant from the NASA Earth Sciences Division, Climate and Radiation program, under H. Maring. The work of R. Kahn is supported in part by the NASA Climate and Radiation Research and Analysis program under H. Maring, the Atmospheric Composition program under Phil DeCola, and the EOS- MISR instrument project. This work was performed at the Jet Propulsion Laboratory, California Institute of Technology, under contract with NASA and at the NASA Goddard Space Flight Center. The MISR data were obtained from the NASA Langley Research Center Atmospheric Sciences Data Center. NR 49 TC 46 Z9 46 U1 0 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 DEC 19 PY 2008 VL 113 AR D24204 DI 10.1029/2008JD010083 PG 17 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 386LC UT WOS:000261883700004 ER PT J AU Lee, T Wang, O Tang, WQ Liu, WT AF Lee, Tong Wang, Ou Tang, Wenqing Liu, W. Timothy TI Wind stress measurements from the QuikSCAT-SeaWinds scatterometer tandem mission and the impact on an ocean model SO JOURNAL OF GEOPHYSICAL RESEARCH-OCEANS LA English DT Article ID INDIAN-OCEAN; SURFACE WIND; SEMIDIURNAL VARIATIONS; PACIFIC-OCEAN; HEAT-FLUX; CIRCULATION; PARAMETERIZATION; VARIABILITY; BOUNDARY; FIELDS AB We examine diurnal signals captured by the QuikSCAT-SeaWinds scatterometer tandem mission (April-October 2003) and their impact on ocean model simulation. The diurnal variability captured by twice-daily scatterometer wind from the tandem mission is substantially larger than that estimated by the National Centers for Environmental Prediction (NCEP) reanalysis product (even with a 6-hourly interval in the latter). Consequently, the impact of diurnal wind on model sea surface temperature (SST) is significantly larger with scatterometer than with NCEP winds because of stronger vertical mixing caused by the twice-daily scatterometer wind. This is consistent with previous studies that high-frequency wind at the ocean's inertial frequencies enhances vertical mixing through resonant inertial oscillations. The weak vertical mixing associated with daily scatterometer winds causes warm bias of SST (relative to that resulting from twice-daily scatterometer wind) and larger deviation from observations. The warm bias reaches several degrees Celsius in midlatitude oceans during summertime and can accumulate with time. Heat flux correction that attempts to account for the feedback of SST would propagate the error in wind and vertical mixing to heat flux without correcting the error source. Because of this error compensation, caution is needed in the interpretation of SST budget resulting from ocean models and data assimilation outputs based on wind products that do not adequately resolve diurnal variability. Our findings highlight the need to resolve diurnal wind in future scatterometer missions. Our study assumes that wind differences between the two scatterometers are primarily due to the sampling of diurnal cycle at different times. However, potential bias between the two needs further investigations. C1 [Lee, Tong; Wang, Ou; Tang, Wenqing; Liu, W. Timothy] CALTECH, Jet Prop Lab, NASA, Pasadena, CA 91109 USA. RP Lee, T (reprint author), CALTECH, Jet Prop Lab, NASA, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM tong.lee@jpl.nasa.gov FU National Aeronautics and Space Administration (NASA); Physical Oceanography Distributed Active Archive Center (PO. DAAC); NASA Jet Propulsion Laboratory, Pasadena, CA FX The research described in this paper was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration (NASA). The scatterometer data used for the analysis were obtained from the Physical Oceanography Distributed Active Archive Center (PO. DAAC) at the NASA Jet Propulsion Laboratory, Pasadena, CA (data are available at http://podaac.jpl.nasa.gov). The model sensitivity experiments were performed on the supercomputers of the JPL Super-computing Project and NASA Ames Research Center. NR 30 TC 8 Z9 8 U1 0 U2 7 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0148-0227 J9 J GEOPHYS RES-OCEANS JI J. Geophys. Res.-Oceans PD DEC 19 PY 2008 VL 113 IS C12 AR C12019 DI 10.1029/2008JC004855 PG 14 WC Oceanography SC Oceanography GA 386LX UT WOS:000261885800002 ER PT J AU Ming, DW Gellert, R Morris, RV Arvidson, RE Brukner, J Clark, BC Cohen, BA d'Uston, C Economou, T Fleischer, I Klingelhofer, G McCoy, TJ Mittlefehldt, DW Schmidt, ME Schroder, C Squyres, SW Treguier, E Yen, AS Zipfel, J AF Ming, D. W. Gellert, R. Morris, R. V. Arvidson, R. E. Bruekner, J. Clark, B. C. Cohen, B. A. d'Uston, C. Economou, T. Fleischer, I. Klingelhoefer, G. McCoy, T. J. Mittlefehldt, D. W. Schmidt, M. E. Schroeder, C. Squyres, S. W. Treguier, E. Yen, A. S. Zipfel, J. TI Geochemical properties of rocks and soils in Gusev Crater, Mars: Results of the Alpha Particle X-Ray Spectrometer from Cumberland Ridge to Home Plate SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Article ID MAGNETIC-PROPERTIES EXPERIMENTS; FLUID INCLUSIONS; SPIRIT ROVER; MINERALOGY; CHEMISTRY; MISSION; DUST AB Geochemical diversity of rocks and soils has been discovered by the Alpha Particle X-Ray Spectrometer ( APXS) during Spirit's journey over Husband Hill and down into the Inner Basin from sol 470 to 1368. The APXS continues to operate nominally with no changes in calibration or spectral degradation over the course of the mission. Germanium has been added to the Spirit APXS data set with the confirmation that it occurs at elevated levels in many rocks and soils around Home Plate. Twelve new rock classes and two new soil classes have been identified at the Spirit landing site since sol 470 on the basis of the diversity in APXS geochemistry. The new rock classes are Irvine ( alkaline basalt), Independence ( low Fe outcrop), Descartes ( outcrop similar to Independence with higher Fe and Mn), Algonquin ( mafic-ultramafic igneous sequence), Barnhill ( volcaniclastic sediments enriched in Zn, Cl, and Ge), Fuzzy Smith ( high Si and Ti rock), Elizabeth Mahon ( high Si, Ni, and Zn outcrop and rock), Halley ( hematite-rich outcrop and rock), Montalva ( high K, hematite-rich rock), Everett ( high Mg, magnetite-rich rock), Good Question ( high Si, low Mn rock), and Torquas ( high K, Zn, and Ni magnetite-rich rock). New soil classes are Gertrude Weise ( very high Si soil) and Eileen Dean ( high Mg, magnetite-rich soil). Aqueous processes have played a major role in the formation and alteration of rocks and soils on Husband Hill and in the Inner Basin. C1 [Ming, D. W.; Morris, R. V.; Mittlefehldt, D. W.; Schroeder, C.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. [Gellert, R.] Univ Guelph, Dept Phys, Guelph, ON N1G 2W1, Canada. [Arvidson, R. E.] Washington Univ, Dept Earth & Planetary Sci, St Louis, MO 63130 USA. [Bruekner, J.] Max Planck Inst Chem, D-55128 Mainz, Germany. [Clark, B. C.] Space Sci Inst, Boulder, CO 80301 USA. [Cohen, B. A.] NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA. [d'Uston, C.; Treguier, E.] Univ Toulouse 3, CNRS, Ctr Etud Spatiale Rayonnements, OMP, F-31028 Toulouse, France. [Economou, T.] Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA. [Fleischer, I.; Klingelhoefer, G.] Johannes Gutenberg Univ Mainz, Inst Anorgan & Analyt Chem, D-55128 Mainz, Germany. [McCoy, T. J.; Schmidt, M. E.] Smithsonian Inst, Dept Mineral Sci, Washington, DC 20560 USA. [Squyres, S. W.] Cornell Univ, Dept Astron, Ithaca, NY 14853 USA. [Yen, A. S.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Zipfel, J.] Forschungsinst, D-60325 Frankfurt, Germany. [Zipfel, J.] Nat Museum Senckenberg, D-60325 Frankfurt, Germany. RP Ming, DW (reprint author), NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. EM douglas.w.ming@nasa.gov RI Schroder, Christian/B-3870-2009; OI Schroder, Christian/0000-0002-7935-6039; Treguier, Erwan/0000-0002-7347-2805 FU NASA; Canadian Space Agency FX We thank the members of the MER project who enable daily science observations at the Spirit landing site. The work described in this paper was conducted at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with NASA. D. W. M. and R. V. M. acknowledge support of the NASA Mars Fundamental Research Program and the NASA Johnson Space Center. R. G. acknowledges support from the Canadian Space Agency. C. S. acknowledges support by an appointment to the NASA Postdoctoral Program at the Johnson Space Center, administered by Oak Ridge Associated Universities through a contract with NASA. We thank David Vaniman and an anonymous reviewer for detailed reviews. NR 44 TC 84 Z9 84 U1 0 U2 26 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 DEC 19 PY 2008 VL 113 IS E12 AR E12S39 DI 10.1029/2008JE003195 PG 28 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 386MH UT WOS:000261886800002 ER PT J AU Ehlmann, BL Mustard, JF Murchie, SL Poulet, F Bishop, JL Brown, AJ Calvin, WM Clark, RN Des Marais, DJ Milliken, RE Roach, LH Roush, TL Swayze, GA Wray, JJ AF Ehlmann, Bethany L. Mustard, John F. Murchie, Scott L. Poulet, Francois Bishop, Janice L. Brown, Adrian J. Calvin, Wendy M. Clark, Roger N. Des Marais, David J. Milliken, Ralph E. Roach, Leah H. Roush, Ted L. Swayze, Gregg A. Wray, James J. TI Orbital Identification of Carbonate-Bearing Rocks on Mars SO SCIENCE LA English DT Article ID MINERALS; CLIMATE; PHYLLOSILICATES; TEMPERATURE; PRODUCTS; SULFATES; OLIVINE; SPECTRA; SYSTEM; MODEL AB Geochemical models for Mars predict carbonate formation during aqueous alteration. Carbonate- bearing rocks had not previously been detected on Mars' surface, but Mars Reconnaissance Orbiter mapping reveals a regional rock layer with near- infrared spectral characteristics that are consistent with the presence of magnesium carbonate in the Nili Fossae region. The carbonate is closely associated with both phyllosilicate- bearing and olivine- rich rock units and probably formed during the Noachian or early Hesperian era from the alteration of olivine by either hydrothermal fluids or near- surface water. The presence of carbonate as well as accompanying clays suggests that waters were neutral to alkaline at the time of its formation and that acidic weathering, proposed to be characteristic of Hesperian Mars, did not destroy these carbonates and thus did not dominate all aqueous environments. C1 [Ehlmann, Bethany L.; Mustard, John F.; Roach, Leah H.] Brown Univ, Dept Geol Sci, Providence, RI 02912 USA. [Murchie, Scott L.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA. [Poulet, Francois] Univ Paris 11, Inst Astrophys Spatiale, F-91405 Orsay, France. [Bishop, Janice L.; Brown, Adrian J.] SETI Inst, Mountain View, CA 94043 USA. [Bishop, Janice L.; Brown, Adrian J.; Des Marais, David J.; Roush, Ted L.] NASA, Ames Res Ctr, Mountain View, CA 94043 USA. [Calvin, Wendy M.] Univ Nevada, Dept Geol Sci & Engn, Reno, NV 89557 USA. [Clark, Roger N.; Swayze, Gregg A.] US Geol Survey, Lakewood, CO 80225 USA. [Milliken, Ralph E.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Wray, James J.] Cornell Univ, Dept Astron, Ithaca, NY 14853 USA. RP Ehlmann, BL (reprint author), Brown Univ, Dept Geol Sci, Providence, RI 02912 USA. RI Wray, James/B-8457-2008; Murchie, Scott/E-8030-2015 OI Wray, James/0000-0001-5559-2179; Murchie, Scott/0000-0002-1616-8751 FU NASA/Keck Reflectance Experiment Laboratory (RELAB) spectral database FX We thank R. Arvidson, R. Morris, N. Mangold, A. Baldridge, J.-P. Bibring, D. Jouglet, A. Fraeman, S. Wiseman, A. McEwen, G. Marzo, P. McGuire, and M. Wyatt for thoughtful discussions during manuscript preparation and E. Cloutis and others who have made quality spectral libraries available and contributed to the building of the NASA/Keck Reflectance Experiment Laboratory (RELAB) spectral database. We are grateful for the ongoing efforts of the MRO science and engineering teams, in particular the CRISM team, which enable these discoveries. NR 45 TC 278 Z9 283 U1 10 U2 63 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 DEC 19 PY 2008 VL 322 IS 5909 BP 1828 EP 1832 DI 10.1126/science.1164759 PG 5 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 385FF UT WOS:000261799400050 PM 19095939 ER PT J AU Hofton, MA Blair, JB Luthcke, SB Rabine, DL AF Hofton, M. A. Blair, J. B. Luthcke, S. B. Rabine, D. L. TI Assessing the performance of 20-25 m footprint waveform lidar data collected in ICESat data corridors in Greenland SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID LASER ALTIMETER; VEGETATION; ACCURACY AB The precision and accuracy of surface elevation measurements of the Greenland ice sheet provided by 20 25 m-footprint waveform laser altimetry is assessed using data collected by NASA's LVIS airborne lidar in September 2007. Repeated data acquisitions from two similar to 850 km long transects over the ice sheet and a similar to 30 km-long transect in the Summit area are evaluated for consistency and compared to in situ data for validation. Comparisons to data collected by NASA's ICESat system reveal good agreement. In the Summit area, differences are better than 0.07 m (1 sigma) (except for L3C where it is 0.13 m), with mean offsets of -0.09 to 0.16 m depending on the campaign. Within the feeder zone to Jakobshavn Glacier, ice elevation decreases of up to 12 m, 2004-2008, are observed. The results suggest that 25 m waveform lidar can measure ice sheet elevation precisely and accurately and that the measurement scheme could be used to complement the legacy ICESat measurements. Citation: Hofton, M. A., J. B. Blair, S. B. Luthcke, and D. L. Rabine (2008), Assessing the performance of 20-25 m footprint waveform lidar data collected in ICESat data corridors in Greenland, Geophys. Res. Lett., 35, L24501, doi: 10.1029/2008GL035774. C1 [Hofton, M. A.] Univ Maryland, Dept Geog, College Pk, MD 20742 USA. [Blair, J. B.; Luthcke, S. B.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Rabine, D. L.] Sci Syst & Applicat Inc, Lanham, MD USA. RP Hofton, MA (reprint author), Univ Maryland, Dept Geog, College Pk, MD 20742 USA. EM Mhofton@umd.edu; Bryan.Blair@nasa.gov; Scott.B.Luthcke@nasa.gov; David.Rabine@nasa.gov RI Khachadourian, Diana/C-8513-2012; Luthcke, Scott/D-6283-2012; Rabine, David/C-9626-2013; Blair, James/D-3881-2013 FU GSFC IRAD; NASA [NNX08AI50G] FX We would like to thank J. Sauber, an anonymous reviewer, R. Bindschadler, R. Ray, E. Frederick, J. Sonntag, J. Yungel, C. Shuman, and B. Hawley. Funding for this project was provided by a GSFC IRAD, and NASA grant NNX08AI50G. The LVIS data are available at https://lvis.gsfc.nasa.gov. NR 10 TC 15 Z9 15 U1 2 U2 9 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD DEC 18 PY 2008 VL 35 IS 24 AR L24501 DI 10.1029/2008GL035774 PG 5 WC Geosciences, Multidisciplinary SC Geology GA 386KO UT WOS:000261882300004 ER PT J AU Jeong, MJ Hsu, NC AF Jeong, Myeong-Jae Hsu, N. Christina TI Retrievals of aerosol single-scattering albedo and effective aerosol layer height for biomass-burning smoke: Synergy derived from "A-Train" sensors SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID SUN AB In this paper, we present results from a new algorithm which provides aerosol layer height (ALH) as well as single-scattering albedo (SSA) for biomass-burning smoke aerosols by merging measurements from three of the "A-Train" satellite sensors: MODIS, OMI, and CALIOP. This algorithm has been applied successfully to biomass burning episodes over North America and Southeast Asia, and the corresponding SSA retrievals show good agreement with those from the AERONET. Furthermore, by combining ALH information from CALIOP with the retrieved SSA, extended information of ALH over wide areas can be obtained outside the CALIPSO track. Even when CALIPSO data are not available, this algorithm will still allow for the separation of aerosols residing within the boundary layer from those elevated in the free troposphere by combining only MODIS and OMI data. Results from this study will provide a better understanding of the height of smoke layers generated from biomass burning and thus improve aerosol models and the prediction of smoke aerosol transport. Citation: Jeong, M.-J., and N. C. Hsu (2008), Retrievals of aerosol single-scattering albedo and effective aerosol layer height for biomass-burning smoke: Synergy derived from "A-Train" sensors, Geophys. Res. Lett., 35, L24801, doi: 10.1029/2008GL036279. C1 [Jeong, Myeong-Jae] Univ Maryland Baltimore Cty, Goddard Earth Sci & Technol Ctr, Baltimore, MD 21228 USA. [Jeong, Myeong-Jae; Hsu, N. Christina] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Jeong, MJ (reprint author), Univ Maryland Baltimore Cty, Goddard Earth Sci & Technol Ctr, Baltimore, MD 21228 USA. EM myeong-jae.jeong-1@nasa.gov RI Jeong, Myeong/B-8803-2008; Hsu, N. Christina/H-3420-2013 FU NASA Applied Sciences Program FX This work is supported by grant from the NASA Applied Sciences Program, under L. Friedl. We thank grant PI John McHenry of Baron Advanced Meteorological Systems for useful discussions during this research. CALIPSO data were obtained from the NASA Langley Research Center Atmospheric Science Data Center. The OMI L1B data were acquired from the Goddard Earth Sciences Distributed Active Archive Center, http://disc.gsfc.nasa.gov. We thank many AERONET principal investigators and their staff for establishing and maintaining the AERONET sites used in this study. We are also grateful to the MODAPS team for producing and distributing the MODIS products. NR 13 TC 21 Z9 21 U1 1 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 DEC 18 PY 2008 VL 35 IS 24 AR L24801 DI 10.1029/2008GL036279 PG 6 WC Geosciences, Multidisciplinary SC Geology GA 386KO UT WOS:000261882300006 ER PT J AU Marzo, GA Roush, TL Blanco, A Fonti, S Orofino, V AF Marzo, G. A. Roush, T. L. Blanco, A. Fonti, S. Orofino, V. TI Statistical exploration and volume reduction of planetary remote sensing spectral data SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Article ID THERMAL EMISSION SPECTROMETER; SURFACE COMPOSITIONS; MARTIAN SURFACE; MGS-TES; MARS; IDENTIFICATION; MINERALS AB Modern planetary scientific experiments are providing a huge amount of information that requires extensive analysis and evaluation in order to understand its scientific content. In this work we evaluate the ability of a previously developed and evaluated technique to explore a large data set in order to identify the cluster representatives of the spectral variability of a selected Martian region and obtain a reduction of the original data volume similar to 2 x 10(4). We also demonstrate that the cluster centroids are able to quantitatively reproduce previously interpreted atmospheric, topographic, and compositional properties. The results build additional confidence in the application of the statistical techniques. C1 [Marzo, G. A.; Roush, T. L.] NASA, Ames Res Ctr, Space Sci & Astrobiol Div, Moffett Field, CA 94035 USA. [Blanco, A.; Fonti, S.; Orofino, V.] Univ Salento, Dept Phys, I-73100 Lecce, Italy. RP Marzo, GA (reprint author), NASA, Ames Res Ctr, Space Sci & Astrobiol Div, Mail Stop 245-3, Moffett Field, CA 94035 USA. EM giuseppe.a.marzo@nasa.gov RI Marzo, Giuseppe/A-9765-2015 FU NASA; Oak Ridge Associated Universities FX This research was supported by an appointment to the NASA Postdoctoral Program at the Ames Research Center, administered by Oak Ridge Associated Universities through a contract with NASA. T. L. R. acknowledges research support from NASA's Planetary Geology and Geophysics Program. NR 30 TC 9 Z9 9 U1 0 U2 1 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 DEC 18 PY 2008 VL 113 IS E12 AR E12009 DI 10.1029/2008JE003219 PG 9 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 386MG UT WOS:000261886700001 ER PT J AU Fairen, AG AF Fairen, Alberto G. TI Finding of unusual soil on Mars could stem from tools used SO NATURE LA English DT Letter C1 [Fairen, Alberto G.] NASA, Ames Res Ctr, Space Sci & Astrogbiol Div, Moffett Field, CA 94035 USA. RP Fairen, AG (reprint author), NASA, Ames Res Ctr, Space Sci & Astrogbiol Div, MS 245-3, Moffett Field, CA 94035 USA. EM afairen@arc.nasa.gov NR 1 TC 0 Z9 0 U1 0 U2 3 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 0028-0836 J9 NATURE JI Nature PD DEC 18 PY 2008 VL 456 IS 7224 BP 870 EP 870 DI 10.1038/456870c PG 1 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 384TY UT WOS:000261768300014 PM 19092906 ER PT J AU Garcia-Comas, M Lopez-Puertas, M Marshall, BT Wintersteiner, PP Funke, B Bermejo-Pantaleon, D Mertens, CJ Remsberg, EE Gordley, LL Mlynczak, MG Russell, JM AF Garcia-Comas, M. Lopez-Puertas, M. Marshall, B. T. Wintersteiner, P. P. Funke, B. Bermejo-Pantaleon, D. Mertens, C. J. Remsberg, E. E. Gordley, L. L. Mlynczak, M. G. Russell, J. M., III TI Errors in Sounding of the Atmosphere using Broadband Emission Radiometry (SABER) kinetic temperature caused by non-local-thermodynamic-equilibrium model parameters SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID CO2 15-MU-M EMISSION; VIBRATIONAL DEACTIVATION; MU-M; COLLISIONAL DEACTIVATION; LOWER THERMOSPHERE; ENERGY-TRANSFER; CARBON-DIOXIDE; ATOMIC OXYGEN; LIMB EMISSION; RATE-CONSTANT AB The vast set of near-global and continuous atmospheric measurements made by the Sounding of the Atmosphere using Broadband Emission Radiometry (SABER) instrument since 2002, including daytime and nighttime kinetic temperature (T-k) from 20 to 105 km, is available to the scientific community. The temperature is retrieved from SABER measurements of the atmospheric 15 mu m CO2 limb emission. This emission separates from local thermodynamic equilibrium (LTE) conditions in the rarefied mesosphere and thermosphere, making it necessary to consider the CO2 vibrational state non-LTE populations in the retrieval algorithm above 70 km. Those populations depend on kinetic parameters describing the rate at which energy exchange between atmospheric molecules take place, but some of these collisional rates are not well known. We consider current uncertainties in the rates of quenching of CO2(v(2)) by N-2, O-2 and O, and the CO2(v(2)) vibrational-vibrational exchange to estimate their impact on SABER T-k for different atmospheric conditions. The T-k is more sensitive to the uncertainty in the latter two, and their effects depend on altitude. The T-k combined systematic error due to non-LTE kinetic parameters does not exceed +/- 1.5 K below 95 km and +/- 4-5 K at 100 km for most latitudes and seasons (except for polar summer) if the T-k profile does not have pronounced vertical structure. The error is +/- 3 K at 80 km, +/- 6 K at 84 km and +/- 18 K at 100 km under the less favorable polar summer conditions. For strong temperature inversion layers, the errors reach +/- 3 K at 82 km and +/- 8 K at 90 km. This particularly affects tide amplitude estimates, with errors of up to +/- 3 K. C1 [Garcia-Comas, M.; Lopez-Puertas, M.; Funke, B.; Bermejo-Pantaleon, D.] CSIC, Inst Astrofis Andalucia, E-18080 Granada, Spain. [Marshall, B. T.; Gordley, L. L.] G & A Tech Software, Newport News, VA 23606 USA. [Mertens, C. J.; Remsberg, E. E.; Mlynczak, M. G.] NASA, Langley Res Ctr, Hampton, VA 23681 USA. [Russell, J. M., III] Hampton Univ, Ctr Atmospher Sci, Hampton, VA 23668 USA. [Wintersteiner, P. P.] ARCON Corp, Waltham, MA 02154 USA. RP Garcia-Comas, M (reprint author), CSIC, Inst Astrofis Andalucia, Apartado Correos 3004, E-18080 Granada, Spain. EM maya@iaa.es; puertas@iaa.es; b.t.marshall@gats-inc.com; winters@arcon.com; bernd@iaa.es; diego@iaa.es; christopher.j.mertens@nasa.gov; ellis.e.remsberg@nasa.gov; l.l.gordley@gats-inc.com; Martin.G.Mlynczak@nasa.gov; james.russell@hamptonu.edu RI Mlynczak, Martin/K-3396-2012; Lopez Puertas, Manuel/M-8219-2013; Garcia-Comas, Maya/E-4050-2014; Funke, Bernd/C-2162-2008 OI Lopez Puertas, Manuel/0000-0003-2941-7734; Garcia-Comas, Maya/0000-0003-2323-4486; Funke, Bernd/0000-0003-0462-4702 FU Spanish project [ESP2004-01556]; EC FEDER; NASA TIMED mission; Air Force Office of Scientific Research FX The IAA team was partially supported by the Spanish project ESP2004-01556 and EC FEDER funds. The SABER science team acknowledges support from NASA TIMED mission under its SABER project. PPW also acknowledges support from Air Force Office of Scientific Research. The authors thank A. K. Smith for her valuable help in the estimation of tidal effects on atomic oxygen, and the anonymous reviewers of this manuscript, who helped to improve its quality with their thoughtful comments and suggestions. NR 42 TC 44 Z9 44 U1 0 U2 1 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 DEC 17 PY 2008 VL 113 AR D24106 DI 10.1029/2008JD010105 PG 16 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 386LA UT WOS:000261883500002 ER PT J AU Schoeberl, MR Douglass, AR Stolarski, RS Pawson, S Strahan, SE Read, W AF Schoeberl, M. R. Douglass, A. R. Stolarski, R. S. Pawson, S. Strahan, S. E. Read, W. TI Comparison of lower stratospheric tropical mean vertical velocities SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID QUASI-BIENNIAL OSCILLATION; TROPOPAUSE TEMPERATURES; ANNUAL CYCLE; WATER-VAPOR; TRANSPORT MODEL; AIR; CIRCULATION; CHEMISTRY; DIAGNOSTICS; ATMOSPHERE AB We have analyzed 13 years (1993-2005) of tropical stratospheric water vapor data from the Halogen Occultation Experiment and over 3 years of data (October 2004 through November 2007) from the Aura Microwave Limb Sounder. By correlating the phase lag of the water vapor "tape recorder'' signal between levels we estimate the time mean vertical velocity. Our estimated vertical velocity compares well with calculations from the Goddard Earth Observing System (GEOS) chemistry-climate model (CCM) and from the GEOS data assimilation system. Between 18 and 26 km both the GEOS CCM simulations and water vapor observations agree that the vertical velocity is below 0.04 cm/s, with a minimum near 20 km of 0.03 cm/s. Vertical velocities deduced from water vapor observations are higher than those from the GEOS CCM in the region 16-18 km (0.04 cm/s) and above 26-30 km (up to 0.07 cm/s). These estimates are close to earlier estimates from a shorter water vapor record and radiative transfer models. No evidence is found for velocities as high as 0.15 cm/s as was recently estimated from aircraft CO2 measurements in the upper troposphere/lower stratosphere. Further diagnosis of the aircraft CO2 data and model simulations of CO2 show that while the CO2 data give an apparent upward transport velocity of similar to 0.06 cm/s, about half of this is due to vertical and horizontal eddy transport. Accounting for the eddy terms gives a CO2-based estimate of the vertical velocity of similar to 0.03 cm/s, in much closer agreement with that estimated from water vapor. C1 [Schoeberl, M. R.; Douglass, A. R.; Stolarski, R. S.; Pawson, S.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Read, W.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Strahan, S. E.] Univ Maryland Baltimore Cty, Goddard Earth Sci & Technol Ctr, Baltimore, MD 21228 USA. RP Schoeberl, MR (reprint author), NASA, Goddard Space Flight Ctr, Mail Stop 613-3,Code 910, Greenbelt, MD 20771 USA. EM mark.r.schoeberl@nasa.gov RI Douglass, Anne/D-4655-2012; Strahan, Susan/H-1965-2012; Stolarski, Richard/B-8499-2013; Pawson, Steven/I-1865-2014 OI Stolarski, Richard/0000-0001-8722-4012; Pawson, Steven/0000-0003-0200-717X FU NASA FX The authors would like to acknowledge funding for this research from the NASA Earth Sciences Program. NR 41 TC 53 Z9 53 U1 0 U2 4 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 DEC 17 PY 2008 VL 113 AR D24109 DI 10.1029/2008JD010221 PG 11 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 386LA UT WOS:000261883500003 ER PT J AU Su, WY Schuster, GL Loeb, NG Rogers, RR Ferrare, RA Hostetler, CA Hair, JW Obland, MD AF Su, Wenying Schuster, Gregory L. Loeb, Norman G. Rogers, Raymond R. Ferrare, Richard A. Hostetler, Chris A. Hair, Johnathan W. Obland, Michael D. TI Aerosol and cloud interaction observed from high spectral resolution lidar data SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID TO-BACKSCATTER RATIO; PARTICLE-PRODUCTION; OPTICAL-PROPERTIES; RAMAN LIDAR; EXTINCTION; MICROPHYSICS; ATMOSPHERE; PRODUCTS; OCEAN; CERES AB Recent studies utilizing satellite retrievals have shown a strong correlation between aerosol optical depth (AOD) and cloud cover. However, these retrievals from passive sensors are subject to many limitations, including cloud adjacency (or three-dimensional) effects, possible cloud contamination, uncertainty in the AOD retrieval. Some of these limitations do not exist in High Spectral Resolution Lidar (HSRL) observations; for instance, HSRL observations are not affected by cloud adjacency effects, are less prone to cloud contamination, and offer accurate aerosol property measurements (backscatter coefficient, extinction coefficient, lidar ratio, backscatter Angstrom exponent, and aerosol optical depth) at a fine spatial resolution (< 100 m) in the vicinity of clouds. Hence the HSRL provides an important data set for studying aerosol and cloud interaction. In this study, we statistically analyze aircraft-based HSRL profiles according to their distance from the nearest cloud, assuring that all profile comparisons are subject to the same largescale meteorological conditions. Our results indicate that AODs from HSRL are about 8 17% higher in the proximity of clouds (similar to 100 m) than far away from clouds (4.5 km), which is much smaller than the reported cloud three-dimensional effect on AOD retrievals. The backscatter and extinction coefficients also systematically increase in the vicinity of clouds, which can be explained by aerosol swelling in the high relative humidity (RH) environment and/or aerosol growth through in-cloud processing (albeit not conclusively). On the other hand, we do not observe a systematic trend in lidar ratio; we hypothesize that this is caused by the opposite effects of aerosol swelling and aerosol in-cloud processing on the lidar ratio. Finally, the observed backscatter Angstrom exponent (BAE) does not show a consistent trend because of the complicated relationship between BAE and RH. We demonstrate that BAE should not be used as a surrogate for Angstrom exponent, especially at high RH. C1 [Su, Wenying; Rogers, Raymond R.; Obland, Michael D.] Sci Syst & Applications Inc, Hampton, VA 23666 USA. [Schuster, Gregory L.; Loeb, Norman G.; Ferrare, Richard A.; Hostetler, Chris A.; Hair, Johnathan W.] NASA, Langley Res Ctr, Hampton, VA 23681 USA. RP Su, WY (reprint author), Sci Syst & Applications Inc, 1 Enterprise Pkwy, Hampton, VA 23666 USA. EM wenying.su-1@nasa.gov FU NASA CALIPSO program FX The authors thank the support from NASA CALIPSO program and NASA Interdisciplinary Research in Earth Science under the direction of Dr. Hal Maring. Wenying Su thanks Bill Smith Jr. for discussions on GOES image. At the time this research was performed, Michael Obland was a NASA postdoctoral fellow at NASA Langley Research Center, administered by Oak Ridge Associated Universities through a contract with NASA. NR 41 TC 45 Z9 49 U1 1 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 DEC 17 PY 2008 VL 113 AR D24202 DI 10.1029/2008JD010588 PG 9 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 386LA UT WOS:000261883500006 ER PT J AU Willis, JK Fu, LL AF Willis, Josh K. Fu, Lee-Lueng TI Combining altimeter and subsurface float data to estimate the time-averaged circulation in the upper ocean SO JOURNAL OF GEOPHYSICAL RESEARCH-OCEANS LA English DT Article ID DEPTH CIRCULATION; STERIC HEIGHT; NORTH PACIFIC; SOUTH-PACIFIC; GULF-STREAM; VARIABILITY; TRANSPORT; LABRADOR; HEAT AB A new technique is presented for estimating time-averaged, upper ocean geostrophic velocity from a combination of altimeter data and subsurface float data. The technique makes uses of the strong relationship between sea-surface height anomaly and anomalous velocity at depth to reduce mesoscale eddy variability in subsurface float displacements. The technique is demonstrated on a region in the North Atlantic that was well sampled by Argo floats. The 2004 through 2006 time-averaged density field was estimated from the surface to 2000 db by combining altimeter and hydrographic data from the floats. In addition, a reference velocity field was estimated at 1000 db based on a combination of altimeter data and subsurface float displacements. The reference velocity field was combined with geostrophic shear based on the density field to produce a three-dimensional estimate of geostrophic velocity from the surface to 2000 db. The Gulf Stream transport in the upper 2000 db is estimated to be 76 Sv at 73 degrees W. In addition, an estimate of the 3-year average dynamic height at the surface was computed by combining the 1000-db reference dynamic height and the time-averaged density field. C1 [Willis, Josh K.; Fu, Lee-Lueng] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Willis, JK (reprint author), CALTECH, Jet Prop Lab, M-S 300-323,4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM jwillis@caltech.edu FU CNES FX The altimeter products were produced by Ssalto/Duacs and distributed by Aviso with support from CNES. Rio05 [Rio and Hernandez, 2004] was produced by the CLS Space Oceanography Division. The 1992 - 2002 mean ocean dynamic topography data has been obtained from Nikolai Maximenko (IPRC) and Peter Niiler (SIO). Thanks to S. Jayne for generously providing his estimate of surface dynamic height. Float data were collected and made freely available by Argo (a pilot program of the Global Ocean Observing System) and contributing national programs (http://www.argo.net/). 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 27 TC 32 Z9 34 U1 0 U2 8 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 DEC 17 PY 2008 VL 113 IS C12 AR C12017 DI 10.1029/2007JC004690 PG 15 WC Oceanography SC Oceanography GA 386LP UT WOS:000261885000002 ER PT J AU Alexeev, II Belenkaya, ES Bobrovnikov, SY Slavin, JA Sarantos, M AF Alexeev, I. I. Belenkaya, E. S. Bobrovnikov, S. Yu. Slavin, J. A. Sarantos, M. TI Paraboloid model of Mercury's magnetosphere SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article ID SOLAR-WIND INTERACTION; MESSENGERS 1ST FLYBY; MAGNETIC-FIELD; HERMEAN MAGNETOSPHERE; TERRESTRIAL PLANETS; SODIUM EXOSPHERE; ELECTRIC-FIELDS; SURFACE; MAGNETOPAUSE; MISSION AB A new "Paraboloidal'' model of Mercury's magnetospheric magnetic field based upon the earlier terrestrial model and using similar techniques is developed. The model describes the field of Mercury's dipole, which is considered to be offset from the planet's center; the magnetopause currents driven by the solar wind; and the tail current system including the cross-tail currents and their closure currents at the magnetopause. The effect of the interplanetary magnetic field (IMF) is modeled as a partial penetration of the IMF into the magnetosphere. The goals of the present work are (1) to develop an easily usable, yet robust model of Mercury's magnetospheric magnetic field and (2) to produce an improved "unified'' determination of Mercury's magnetic dipole moment which fits the measurements taken during both Mariner 10's first and third flybys. This new model of Mercury's magnetosphere is described and used to determine a best Mercury magnetic dipole moment of 192 nT R-M(3), from the two Mariner 10 flybys, a value which is intermediate between the various estimates produced by previous models. The best fit to the Mariner 10 measurements gives the dipole offset 0.18 R-M above the equatorial plane. The new Paraboloidal model is used to predict the configuration of this miniature magnetosphere under average and extreme solar wind conditions. C1 [Alexeev, I. I.; Belenkaya, E. S.; Bobrovnikov, S. Yu.] Moscow MV Lomonosov State Univ, Inst Nucl Phys, Moscow, Russia. [Slavin, J. A.; Sarantos, M.] NASA, GSFC, Heliophys Sci Div, Greenbelt, MD 20771 USA. RP Alexeev, II (reprint author), Moscow MV Lomonosov State Univ, Inst Nucl Phys, POB 119991, Moscow, Russia. EM james.a.slavin@nasa.gov RI Belenkaya, Elena/D-6940-2012; Slavin, James/H-3170-2012; Alexeev, Igor/G-8773-2011; Sarantos, Menelaos/H-8136-2013 OI Slavin, James/0000-0002-9206-724X; FU RFBR [07-05-00529]; NASA FX Work at the Institute of Nuclear Physics, Moscow State University, was supported by the RFBR Grant 07-05-00529. MS was supported by the NASA Postdoctoral Program (NPP).; Wolfgang Baumjohann thanks the reviewers for their assistance in evaluating this paper. NR 76 TC 31 Z9 32 U1 2 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 DEC 17 PY 2008 VL 113 IS A12 AR A12210 DI 10.1029/2008JA013368 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 386MQ UT WOS:000261887700001 ER PT J AU Liston, DB Stone, LS AF Liston, Dorion B. Stone, Leland S. TI Effects of Prior Information and Reward on Oculomotor and Perceptual Choices SO JOURNAL OF NEUROSCIENCE LA English DT Article DE saccade; attention; basal ganglia; superior colliculus; frontal eye field; lateral intraparietal area ID FRONTAL EYE FIELD; SUPERIOR COLLICULUS; SPATIAL ATTENTION; CAUDATE-NUCLEUS; RESPONSE BIAS; VISUAL-SEARCH; AREA V4; MACAQUE; MOVEMENTS; DECISION AB Expectations about the environment influence motor behavior. In simple tasks, for example, prior knowledge about which stimulus event will likely occur or which response will likely be rewarded induces a tendency to take the favored action (i.e., a motor or response bias), especially when sensory information is sparse or ambiguous. Models of choice behavior account for this bias by weighting decision alternatives unequally, either at an early sensory-input stage or at a downstream motor-output stage. These two alternatives can be distinguished empirically; the former predicts an altered percept that correlates with motor bias, the latter predicts no perceptual effect. By varying the prior probability of target or reward location, we induced biased oculomotor responses in a brightness selection task with human subjects. We found that the induced motor bias was correlated with an amplification of both the sensory signals and internal noise underlying brightness perception, without a systematic change in perceived overall brightness. We also found that the magnitude of the sensory amplification was correlated with the amount of noise in the brightness percept, consistent with a multiplicative weighting factor located downstream from the limiting internal sensory noise. Our data demonstrate that prior knowledge (about target location or reward) shapes visual signals for perception and action in parallel but does not improve the quality (i.e., signal-to-noise ratio) of sensory processing. C1 [Liston, Dorion B.; Stone, Leland S.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Liston, Dorion B.] San Jose State Univ, San Jose, CA 95192 USA. RP Liston, DB (reprint author), NASA, Ames Res Ctr, Mail Stop 262-2, Moffett Field, CA 94035 USA. EM dorion.b.liston@nasa.gov FU NASA's Space Human Factors Engineering Program FX This work was supported by NASA's Space Human Factors Engineering Program. We are grateful to Al Ahumada for suggesting the continuous analysis and to Miguel Eckstein, Brent Beutter, and Barbara Chapman for helpful feedback on a previous draft of this manuscript. We also thank the two anonymous reviewers for their insightful feedback and helpful suggestions and Rami Ersheid for technical support. NR 58 TC 33 Z9 33 U1 0 U2 2 PU SOC NEUROSCIENCE PI WASHINGTON PA 11 DUPONT CIRCLE, NW, STE 500, WASHINGTON, DC 20036 USA SN 0270-6474 J9 J NEUROSCI JI J. Neurosci. PD DEC 17 PY 2008 VL 28 IS 51 BP 13866 EP 13875 DI 10.1523/JNEUROSCI.3120-08.2008 PG 10 WC Neurosciences SC Neurosciences & Neurology GA 384YM UT WOS:000261780100016 PM 19091976 ER PT J AU Rind, D Lean, J Lerner, J Lonergan, P Leboissitier, A AF Rind, D. Lean, J. Lerner, J. Lonergan, P. Leboissitier, A. TI Exploring the stratospheric/tropospheric response to solar forcing SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID SEA-SURFACE TEMPERATURE; TROPOSPHERE-STRATOSPHERE SYSTEM; UV VARIABILITY; CLIMATE VARIATIONS; OCEAN TEMPERATURE; EARTHS ATMOSPHERE; CYCLE VARIABILITY; JULY-AUGUST; SIGNAL; OZONE AB We use the new Goddard Institute for Space Studies Global Climate Middle Atmosphere Model 3 with four different resolutions to investigate various aspects of solar cycle influence on the troposphere/stratosphere system. Three different configurations of sea surface temperatures are used to help determine whether the tropospheric response is due to forcing from above (UV variations impacting the stratosphere) or below (total solar irradiance changes acting through the surface temperature field). The results show that the stratospheric response is highly repeatable and significant. With the more active sun, the annual residual circulation change features relative increased upwelling in the Southern Hemisphere and downwelling in the Northern Hemisphere. Stratospheric west wind increases extend down into the troposphere, especially during Southern Hemisphere winter, and in some runs the jet stream weakens and moves poleward. The predominant tropospheric response consists of warming in the troposphere, with precipitation decreases south of the equator and in the Northern Hemisphere subtropics and midlatitudes, with increases north of the equator especially over southern Asia. The tropospheric response is often not significant, but is fairly robust among the different simulations. These features, which have been reported in observations and other model studies, appear to be driven both from the stratosphere and the surface; nevertheless, they account for only a small percentage of the total variance. More accurate simulations of the solar cycle stratospheric ozone response, the quasi-biennial oscillation, and coupled atmosphere-ocean dynamics are necessary before any conclusions can be deemed definitive. C1 [Rind, D.] Columbia Univ, NASA, Goddard Inst Space Studies, New York, NY 10025 USA. [Lean, J.] USN, Res Lab, Washington, DC 20375 USA. [Lerner, J.; Lonergan, P.; Leboissitier, A.] Columbia Univ, Ctr Climate Syst Res, New York, NY 10025 USA. RP Rind, D (reprint author), Columbia Univ, NASA, Goddard Inst Space Studies, 2880 Broadway, New York, NY 10025 USA. EM drind@giss.nasa.gov OI Lean, Judith/0000-0002-0087-9639 FU NASA FX This work was supported by the NASA Living With A Star program and the NASA Atmospheric Composition focus area. Computer time was provided by the NASA NCCS high-speed computing program. Climate modeling at GISS in general is supported by the NASA Climate Variability and Climate Change focus area. NR 63 TC 45 Z9 51 U1 2 U2 13 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 DEC 16 PY 2008 VL 113 AR D24103 DI 10.1029/2008JD010114 PG 25 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 386KY UT WOS:000261883300003 ER PT J AU Farrand, WH Bell, JF Johnson, JR Arvidson, RE Crumpler, LS Hurowitz, JA Schroder, C AF Farrand, W. H. Bell, J. F., III Johnson, J. R. Arvidson, R. E. Crumpler, L. S. Hurowitz, J. A. Schroder, C. TI Rock spectral classes observed by the Spirit Rover's Pancam on the Gusev Crater Plains and in the Columbia Hills SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Article ID MARS; HEMATITE; ANALOG; SOIL AB This paper examines the ferrous and ferric iron mineralogy of rocks inferred from 246 visible/near-infrared (430-1010 nm) multispectral observations made by the Mars Exploration Rover Spirit's Pancam on its traverse from its landing site to its second Winter Haven location. Principal component, correspondence analyses, and a sequential maximum angle convex cone technique were used to identify 14 candidate classes. Spectra from the West Spur of Husband Hill and the Watchtower area had the highest 535 and 601 nm band depths indicating that these areas were more oxidized. Differences in the depth and band center of a near infrared (NIR) absorption feature were observed using 904 nm band depth and 803: 904 nm ratio and parameters gauging the 754-864 and 754-1009 nm slopes. Spectra of rocks from the southern flank of Husband Hill had negative 754-1009 nm slopes and a broad NIR absorption consistent with high olivine abundances. Rocks observed on the lower West Spur, at the Cumberland Ridge locale, at the Husband Hill summit, and at the Haskin Ridge locale had deep 904 nm band depths and steep 754-864 nm slopes consistent with greater pyroxene abundances. These observations are consistent with results on iron-bearing mineralogy from Spirit's Mossbauer spectrometer. Comparisons of these rock spectral classes with a set of terrestrial analog samples found similarities between the West Spur and Watchtower classes and red hematite-bearing impact melts. Fewer similarities were found in comparisons of the Columbia Hills classes with basaltic hydrovolcanic tephras. C1 [Farrand, W. H.] Space Sci Inst, Boulder, CO 80301 USA. [Bell, J. F., III] Cornell Univ, Dept Astron, Ithaca, NY 14853 USA. [Johnson, J. R.] US Geol Survey, Astrogeol Team, Flagstaff, AZ 86001 USA. [Arvidson, R. E.] Washington Univ, Dept Earth & Planetary Sci, St Louis, MO 63130 USA. [Crumpler, L. S.] New Mexico Museum Nat Hist & Sci, Albuquerque, NM 87104 USA. [Hurowitz, J. A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Schroder, C.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. RP Farrand, WH (reprint author), Space Sci Inst, 4750 Walnut St,Suite 205, Boulder, CO 80301 USA. EM farrand@spacescience.org RI Schroder, Christian/B-3870-2009; Johnson, Jeffrey/F-3972-2015 OI Schroder, Christian/0000-0002-7935-6039; NR 51 TC 24 Z9 24 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 DEC 16 PY 2008 VL 113 IS E12 AR E12S38 DI 10.1029/2008JE003237 PG 25 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 386ME UT WOS:000261886500001 ER PT J AU Prather, MJ Zhua, X Strahan, SE Steenrod, SD Rodriguez, JM AF Prather, Michael J. Zhua, Xin Strahan, Susan E. Steenrod, Stephen D. Rodriguez, Jose M. TI Quantifying errors in trace species transport modeling SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF AMERICA LA English DT Article DE biogeochemical cycles; model errors; source inversions; uncertainties ID GENERAL-CIRCULATION MODEL; ATMOSPHERIC TRANSPORT; NUMERICAL ADVECTION; INITIATIVE ASSESSMENT; CO2; CHEMISTRY; FORMULATIONS; SIMULATIONS; SENSITIVITY; DYNAMICS AB One expectation when computationally solving an Earth system model is that a correct answer exists, that with adequate physical approximations and numerical methods our solutions will converge to that single answer. With such hubris, we performed a controlled numerical test of the atmospheric transport of CO2 using 2 models known for accurate transport of trace species. Resulting differences were unexpectedly large, indicating that in some cases, scientific conclusions may err because of lack of knowledge of the numerical errors in tracer transport models. By doubling the resolution, thereby reducing numerical error, both models show some convergence to the same answer. Now, under realistic conditions, we identify a practical approach for finding the correct answer and thus quantifying the advection error. C1 [Prather, Michael J.; Zhua, Xin] Univ Calif Irvine, Earth Syst Sci Dept, Irvine, CA 92697 USA. [Strahan, Susan E.; Steenrod, Stephen D.] Univ Maryland Baltimore Cty, Goddard Earth Sci & Technol Ctr, Greenbelt, MD 20771 USA. [Rodriguez, Jose M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Prather, MJ (reprint author), Univ Calif Irvine, Earth Syst Sci Dept, 3329 Croul Hall, Irvine, CA 92697 USA. EM mprather@uci.edu RI Strahan, Susan/H-1965-2012; Steenrod, Stephen/H-2218-2012 FU National Aeronautics and Space Administration [NNG06GB84G, NNG04GA09G]; National Science Foundation [NSF ATM-0550234]; Kavli Foundation FX We thank 2 referees for their insightful comments. This work was supported at the University of California, Irvine, by National Aeronautics and Space Administration Grants NNG06GB84G and NNG04GA09G, National Science Foundation Grant NSF ATM-0550234, and the Kavli Foundation. NR 30 TC 28 Z9 28 U1 1 U2 4 PU NATL ACAD SCIENCES PI WASHINGTON PA 2101 CONSTITUTION AVE NW, WASHINGTON, DC 20418 USA SN 0027-8424 J9 P NATL ACAD SCI USA JI Proc. Natl. Acad. Sci. U. S. A. PD DEC 16 PY 2008 VL 105 IS 50 BP 19617 EP 19621 DI 10.1073/pnas.0806541106 PG 5 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 385GI UT WOS:000261802300011 PM 19066224 ER PT J AU Levine, LH Kasahara, H Kopka, J Erban, A Fehrl, I Kaplan, F Zhao, W Littell, RC Guy, C Wheeler, R Sager, J Mills, A Levine, HG AF Levine, Lanfang H. Kasahara, Hirokazu Kopka, Joachim Erban, Alexander Fehrl, Ines Kaplan, Fatma Zhao, Wei Littell, Ramon C. Guy, Charles Wheeler, Raymond Sager, John Mills, Aaron Levine, Howard G. TI Physiologic and metabolic responses of wheat seedlings to elevated and super-elevated carbon dioxide SO ADVANCES IN SPACE RESEARCH LA English DT Article DE Elevated carbon dioxide; Evapotranspiration (ET); Metabolite profile; Primary metabolites; Secondary metabolites; Super-elevated carbon dioxide; Wheat (Triticum aestivum) ID CHROMATOGRAPHY-MASS SPECTROMETRY; CO2 ENRICHMENT; STOMATAL CONDUCTANCE; FEEDBACK-REGULATION; LEAF SENESCENCE; GENE-EXPRESSION; ATMOSPHERIC CO2; LOTUS-JAPONICUS; PHOTOSYNTHESIS; ACCLIMATION AB The metabolic consequence Of suboptimal (400 mu mol mol(-1) or ppm), near-optimal (1500 ppm)and supra-optimal (10,000 ppm) atmospheric carbon dioxide concentrations [CO(2)] Wits investigated in an attempt to reveal plausible underlying mechanisms for the differential physiological and developmental responses to increasing [CO(2)] Both non-targeted and targeted metabolite profiling by GC-MS and LC-MS were employed to examine primary and secondary metabolites in wheat (Triticum aestivum, cv Yocoro rojo) continuously exposed to these [CO(2)] levels for 14, 21 and 28 days. Metabolite profile wits altered by both [CO(2)] and physiological age. In general, plants grown under high [CO(2)] exhibited a metabolite profile characteristic of older plants under ambient CO(2) Elevated [CO(2)] resulted in higher levels of phosphorylated sugar intermediates, though no clear trend in the content of reducing sugars was observed. Transient starch content was enhanced by increasing [CO(2)] to it Much greater extent at 10,000 ppm CO(2) than at 1500 ppm CO(2). The percentage increase of starch content resulting from CO(2) enrichment declined as plants develope. In contrast, elevated [CO(2)] promoted the accumulation of secondary metabolites (flavonoids) progressively to it greater extent as plants became mature. Elevated [CO(2)] to 1500 ppm induced it higher initial growth rate, while super-elevated [CO(2)] appeared to negate such initial growth promotion. However, after 4 weeks, there was no difference in vegetative growth between 1500 and 10,000 ppm CO(2)-grown plants, both elevated CO(2) levels resulted in all overall 25% increase in biomass over the control plants. More interestingly, elevated atmospheric [CO(2)] reduced evapotranspiration rate (ET), but further increase to the supra-optimal level resulted in increased ET (it reversed trend), i.e. ET at 1500 ppm < ET at 10,000 ppm < ET at 400 ppm. the differential effect of elevated and super-elevated CO(2) oil plants was further reflected in the nitrogen dynamics. These results provide the potential metabolic basis for the differential productivity and stomatal function of plants grown under elevated and super-elevated CO(2) levels. (C) 2008 COSPAR. Published by Elsevier Ltd. All rights reserved. C1 [Levine, Lanfang H.] Dynamac Corp, Space Life Sci Lab, Kennedy Space Ctr, FL 32899 USA. [Kasahara, Hirokazu] Hokkaido Tokai Univ, Sch Engn, Dept Biosci & Technol, Sapporo, Hokkaido, Japan. [Kopka, Joachim; Erban, Alexander; Fehrl, Ines] Max Planck Inst Mol Pflanzenphysiol, D-14476 Golm, Germany. [Kaplan, Fatma; Guy, Charles] Univ Florida, Dept Environm Hort, Plant Mol & Cellular Biol Program, Gainesville, FL 32611 USA. [Zhao, Wei; Littell, Ramon C.] Univ Florida, Inst Food & Agr Sci, Dept Stat, Gainesville, FL 32611 USA. [Wheeler, Raymond; Sager, John; Mills, Aaron; Levine, Howard G.] NASA, Sustainable Syst Div, Kennedy Space Ctr, FL 32899 USA. RP Levine, LH (reprint author), Dynamac Corp, Space Life Sci Lab, Kennedy Space Ctr, FL 32899 USA. EM lanfang.h.levine@nasa.gov OI Kopka, Joachim/0000-0001-9675-4883 FU NASA NRA [NCC 10-5, NAG10-316]; KSC Center Director Discretionary Fund FX We acknowledge Gerogiana Tynes for her assistance in plant cultivation and sampling. This work was supported by: (1) NASA NRA Grant NCC 10-5, (2) it metabolomics initiative via SABRE/UF from NASA Grant NAG10-316, and (3) the KSC Center Director Discretionary Fund 2005. NR 51 TC 21 Z9 24 U1 1 U2 15 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 0273-1177 J9 ADV SPACE RES JI Adv. Space Res. PD DEC 15 PY 2008 VL 42 IS 12 BP 1917 EP 1928 DI 10.1016/j.asr.2008.07.014 PG 12 WC Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences GA 384FD UT WOS:000261728800005 ER PT J AU Drysdale, A Nakamura, T Yorio, N Sager, J Wheeler, R AF Drysdale, Alan Nakamura, Takashi Yorio, Neil Sager, John Wheeler, Ray TI Use of sunlight for plant lighting in a bioregenerative life support system - Equivalent system mass calculations SO ADVANCES IN SPACE RESEARCH LA English DT Article DE Space life sciences; Bioregenerative systems; Plant lighting systems AB Plant lighting is it critical issue for cost effectiveness of bioregenerative systems. A plant lighting system using sunlight has been investigated and compared to systems using electrical lighting. Co-generation of electricity and use of in situ resource utilization (ISRU) were also considered. The fixed part of equivalent system mass was found to be reduced by factors of from 3.1 to 3.9, according to the mission assumptions. The time-dependent part of equivalent system mass was reduced by it smaller value, of about 1.05. Cost effectiveness of bioregeneration hits been compared to the cost of shipping food. Break-even times for different Lunar and Mars missions were generally in the order of 2-10 years, and were quite sensitive to the assumptions. There is significant scope for future refinement of these values, and work is ongoing. (C) 2008 COSPAR. Published by Elsevier Ltd. All rights reserved. C1 [Nakamura, Takashi] Phys Sci Inc, New England Business Ctr 20, Andover, MA 01810 USA. [Yorio, Neil] Dynamac Corp, DYN 3, Kennedy Space Ctr, FL 32815 USA. [Sager, John; Wheeler, Ray] NASA, Kennedy Space Ctr, FL 32815 USA. RP Drysdale, A (reprint author), 6208 Windover Way, Titusville, FL 32780 USA. EM gnrlact@cfl.rr.com; nakamura@psicorp.com; neil.c.yorio@nasa.gov; john.c.sager@nasa.gov; raymond.m.wheeler@nasa.gov FU SBIR [NNK060M15C] FX This work was supported by SBIR Grant NNK060M15C. NR 25 TC 4 Z9 4 U1 0 U2 5 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 0273-1177 J9 ADV SPACE RES JI Adv. Space Res. PD DEC 15 PY 2008 VL 42 IS 12 BP 1929 EP 1943 DI 10.1016/j.asr.2008.09.020 PG 15 WC Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences GA 384FD UT WOS:000261728800006 ER PT J AU Ito, M Messenger, S AF Ito, Motoo Messenger, Scott TI Isotopic imaging of refractory inclusions in meteorites with the NanoSIMS 50L SO APPLIED SURFACE SCIENCE LA English DT Article DE NanoSIMS 50L; Ca, Al-rich inclusions (CAIs); Oxygen isotope image; Isotopic measurement; Cooling rate; Extraterrestrial material ID AL-RICH INCLUSIONS; SOLAR-SYSTEM; ALLENDE; ORIGIN; CA; ANOMALIES; HETEROGENEITY; CHONDRITES; NEBULA; RATIOS AB Oxygen isotopic micro-distributions within and among silicate and oxide minerals in a meteorite were measured with the JSC NanoSIMS 50L by isotopic imaging. High precision isotopic images with micrometer-scale resolution revealed detailed O isotope distributions within CAI minerals. Small-scale heterogeneous distributions of O isotopes constrain the history of isotopic exchange mechanisms in the CAI during and since its formation in the early solar system. We describe the development O isotopic imaging of insulating minerals with high precision of +/-6 and 3 parts per thousand for delta(17)O and delta(18)O, respectively. Published by Elsevier B.V. C1 [Ito, Motoo; Messenger, Scott] NASA, Lyndon B Johnson Space Ctr, ARES, Robert M Walker Lab Space Sci, Houston, TX 77573 USA. RP Ito, M (reprint author), NASA, Lyndon B Johnson Space Ctr, ARES, Robert M Walker Lab Space Sci, 2101 NASA Pkwy, Houston, TX 77573 USA. EM motoo.ito-1@nasa.gov; scott.r.messenger@nasa.gov NR 28 TC 5 Z9 5 U1 0 U2 7 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0169-4332 J9 APPL SURF SCI JI Appl. Surf. Sci. PD DEC 15 PY 2008 VL 255 IS 4 BP 1446 EP 1450 DI 10.1016/j.apsusc.2008.05.095 PG 5 WC Chemistry, Physical; Materials Science, Coatings & Films; Physics, Applied; Physics, Condensed Matter SC Chemistry; Materials Science; Physics GA 460UX UT WOS:000267217500062 ER PT J AU Solaimanzadeh, I Schlegel, TT Feiveson, AH Greco, EC Depalma, JL Starc, V Marthol, H Tutaj, M Buechner, S Axelrod, FB Hilz, MJ AF Solaimanzadeh, I. Schlegel, T. T. Feiveson, A. H. Greco, E. C. Depalma, J. L. Starc, V. Marthol, H. Tutaj, M. Buechner, S. Axelrod, F. B. Hilz, M. J. TI Advanced electrocardiographic predictors of mortality in familial dysautonomia SO AUTONOMIC NEUROSCIENCE-BASIC & CLINICAL LA English DT Article DE Heart rate variability; Bradycardia; Signal averaged ECG; QT interval; QRS-T angle; T-wave morphology; Hypoxia; Left ventricular hypertrophy ID LEFT-VENTRICULAR HYPERTROPHY; HEART-RATE-VARIABILITY; OBSTRUCTIVE SLEEP-APNEA; QT INTERVAL VARIABILITY; SUDDEN CARDIAC DEATH; T-WAVE MORPHOLOGY; MYOCARDIAL-INFARCTION; BLOOD-PRESSURE; REPOLARIZATION LABILITY; ATRIOVENTRICULAR-BLOCK AB Objective: To identify electrocardiographic predictors of mortality in patients with familial dysautonomia (FD). Methods: Ten-minute resting high-fidelity 12-lead electrocardiograms (ECGs) were obtained from 14 FD patients and 14 age/gender-matched healthy subjects. Multiple conventional and advanced ECG parameters were Studied for their ability to predict mortality over a subsequent 4.5-year period, including representative parameters of heart rate variability (HRV), QT variability (QTV), T-wave complexity, signal averaged ECG, and 3-dimensional ECG. Results: Four of the 14 FD patients died during the follow-up period, three with concomitant pulmonary disorder. Of the ECG parameters Studied, increased non-HRV-correlated QTV and decreased HRV were the most predictive of death. Compared to controls as a group, FD patients also had significantly increased ECG voltages. JTc intervals and waveform complexity, suggggestive of structural heart disease. Conclusion: Increased QTV and decreased HRV are markers for increased risk of death in FD patients. When present, both markets may reflect concurrent pathological processes, especially hypoxia due to pulmonary disorders and sleep apnea. C1 [Schlegel, T. T.; Feiveson, A. H.; Greco, E. C.; Depalma, J. L.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. [Solaimanzadeh, I.] Natl Space Biomed Res Inst, Houston, TX USA. [Solaimanzadeh, I.] CUNY Queens Coll, Flushing, NY USA. [Starc, V.] Univ Ljubljana, Inst Physiol, Ljubljana, Slovenia. [Marthol, H.] Univ Erlangen Nurnberg, Dept Neurol, D-8520 Erlangen, Germany. [Tutaj, M.] Jagiellonian Univ, Dept Neurol, Krakow, Poland. [Buechner, S.] Reg Gen Hosp, Dept Neurol, Bolzano, Italy. [Axelrod, F. B.; Hilz, M. J.] NYU, Med Ctr, Dept Neurol, New York, NY 10016 USA. RP Schlegel, TT (reprint author), NASA, Lyndon B Johnson Space Ctr, Mail Code SK3, Houston, TX 77058 USA. EM todd.t.schlegel@nasa.gov FU National Space Biomedical Research Institute; Johnson Space Center Technology Investment Fund; Johnson Space Center Summer Faculty Fellowship; USA-Slovenia Cooperation in Science and Technology; Kosciuszko Foundation; Dysautonomia Foundation, Inc. FX This research was supported by grants front the National Space Biomedical Research Institute (Student Internship Program, Mr. Solaimanzadeh), the Johnson Space Center Technology Investment Fund (Dr. Schlegel), the Johnson Space Center Summer Faculty Fellowship program (Drs. Greco and DePalma), the USA-Slovenia Cooperation in Science and Technology (Drs. Starc and Schlegel), the Kosciuszko Foundation (Dr. Tutaj), and the Dysautonomia Foundation, Inc. (Drs. Axelrod, Hilz, Marthol, Buechner). The advanced ECG hardware and software were provided Courtesy of CardioSoft and Enhanced Cardiology, Houston, TX. NR 70 TC 16 Z9 16 U1 1 U2 1 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 1566-0702 J9 AUTON NEUROSCI-BASIC JI Auton. Neurosci-Basic Clin. PD DEC 15 PY 2008 VL 144 IS 1-2 BP 76 EP 82 DI 10.1016/j.autneu.2008.08.016 PG 7 WC Neurosciences SC Neurosciences & Neurology GA 386BM UT WOS:000261857300009 PM 18851930 ER PT J AU Sawakuchi, GO Yukihara, EG McKeever, SWS Benton, ER Gaza, R Uchihori, Y Yasuda, N Kitamura, H AF Sawakuchi, G. O. Yukihara, E. G. McKeever, S. W. S. Benton, E. R. Gaza, R. Uchihori, Y. Yasuda, N. Kitamura, H. TI Relative optically stimulated luminescence and thermoluminescence efficiencies of Al2O3:C dosimeters to heavy charged particles with energies relevant to space and radiotherapy dosimetry SO JOURNAL OF APPLIED PHYSICS LA English DT Article DE aerospace biophysics; alumina; carbon; dosimetry; photoluminescence; radiation therapy; thermoluminescent dosimeters ID THERMO-LUMINESCENCE; RADIATION-DOSIMETRY; OSL; ION; DETECTORS; TRACK; LIF; IRRADIATION; STATION; SYSTEM AB This article presents a comprehensive characterization of the thermoluminescence (TL) and optically stimulated luminescence (OSL) relative luminescence efficiencies of carbon-doped aluminum (Al2O3:C) for heavy charged particles (HCPs) with atomic numbers ranging from 1 (proton) to 54 (xenon) and energies ranging from 7 to 1000 MeV/u, and investigates the dependence of the Al2O3:C response on experimental conditions. Relative luminescence efficiency values are presented for 19 primary charge/energy combinations, plus 31 additional charge/energy combinations obtained by introducing absorbers in the primary beam. Our results show that for energies of hundreds of MeV/u the data can be described by a single curve of relative luminescence efficiency versus linear energy transfer (LET). This information is needed to compensate for the reduced OSL efficiency to high-LET particles in such applications as space dosimetry. For lower energies, the relative luminescence efficiency as function of LET cannot be described by a single curve; instead, it separates into different components corresponding to different particles. We also present data on the low-LET dose response of Al2O3:C, measured under the same experimental conditions in which the relative luminescence efficiencies to HCPs were obtained, providing information relevant to future theoretical investigations of HCP energy deposition and luminescence production in Al2O3:C. C1 [Uchihori, Y.; Yasuda, N.; Kitamura, H.] Natl Inst Radiol Sci, Chiba 2638555, Japan. [Sawakuchi, G. O.; Yukihara, E. G.; McKeever, S. W. S.; Benton, E. R.] Oklahoma State Univ, Dept Phys, Radiat Dosimetry Lab, Stillwater, OK 74078 USA. [Gaza, R.] Univ Space Res Assoc, Div Space Life Sci, Houston, TX 77058 USA. [Gaza, R.] NASA, Lyndon B Johnson Space Ctr, Space Radiat Anal Grp, Houston, TX 77058 USA. RP Sawakuchi, GO (reprint author), Univ Texas MD Anderson Canc Ctr, Dept Radiat Phys, Unit 94,1515 Holcombe Blvd, Houston, TX 77030 USA. EM gsawakuchi@mdanderson.org; eduardo.yukihara@okstate.edu RI Sawakuchi, Gabriel/A-8961-2009; Yukihara, Eduardo/F-1345-2014 OI Yukihara, Eduardo/0000-0002-4615-6698 NR 52 TC 18 Z9 18 U1 2 U2 14 PU AMER INST PHYSICS PI MELVILLE PA CIRCULATION & FULFILLMENT DIV, 2 HUNTINGTON QUADRANGLE, STE 1 N O 1, MELVILLE, NY 11747-4501 USA SN 0021-8979 J9 J APPL PHYS JI J. Appl. Phys. PD DEC 15 PY 2008 VL 104 IS 12 AR 124903 DI 10.1063/1.3041655 PG 10 WC Physics, Applied SC Physics GA 391HT UT WOS:000262225100127 ER PT J AU Gruszczynski, M Marshall, JD Goldring, R Coleman, ML Malkowski, K Gazdzicka, E Semil, J Gatt, P AF Gruszczynski, Michal Marshall, Jim D. Goldring, Roland Coleman, Max L. Malkowski, Krzysztof Gazdzicka, Elzbieta Semil, Julia Gatt, Peter TI Hiatal surfaces from the Miocene Globigerina Limestone Formation of Malta: Biostratigraphy, sedimentology, trace fossils and early diagenesis SO PALAEOGEOGRAPHY PALAEOCLIMATOLOGY PALAEOECOLOGY LA English DT Article; Proceedings Paper CT Symposium on Biotic-Sediment Interactions in honor of Roland Goldring CY JUL 20-22, 2006 CL Univ Reading, Reading, ENGLAND SP Ichron Ltd, BG Grp, Palaeontol Assoc HO Univ Reading DE Hardgrounds and firmgrounds; Carbon and oxygen stable isotopes; Calcite and dolomite cementation ID CALCAREOUS NANNOFOSSIL BIOSTRATIGRAPHY; ORDOVICIAN HARDGROUND COMMUNITY; ISLAND SOUND SEDIMENTS; SUBMARINE LITHIFICATION; MEDITERRANEAN REGION; CARBONATE SEDIMENTS; BEAR-ISLAND; ENVIRONMENTS; BASIN; SEA AB The Miocene Globigerina Limestone of the Maltese islands contains widespread omission surfaces with very different characteristics and origins. The terminal Lower Globigerina Limestone hardground (TLGLHg) formed during a period of falling sea level. Coccolith assemblages suggest shallowness. Sedimentary structures and trace fossil assemblages, indicate increasing frequency of storm events and erosional episodes, towards the surface. Calcite cementation which took place around Thalassinoides burrows and formed irregular nodules was followed by dissolution of aragonite. It is suggested that lithification was linked to microbial reactions involving organic matter. In contrast two later surfaces, the terminal Middle Globigerina Limestone omissionground (TMGLOg), which marks the Lower to Middle Miocene boundary, and the Fomm-ir-Rih local hardground (FiRLHg) both contain early diagenetic dolomite. Lithification took place in two phases. The dolomite is interpreted to have formed beneath the sea floor: it was subsequently exhumed and partially corroded as the precipitation of calcitic and phosphatic cements took place around burrows open to the circulation of sea water. (C) 2008 Elsevier B.V. All rights reserved. C1 [Gruszczynski, Michal] Uniwersytet Jana Kochanowskiego, Inst Geog, PL-25406 Kielce, Poland. [Gruszczynski, Michal; Malkowski, Krzysztof] Polish Acad Sci, Inst Paleobiol, PL-00818 Warsaw, Poland. [Marshall, Jim D.] Univ Liverpool, Liverpool L69 3GP, Merseyside, England. [Goldring, Roland; Coleman, Max L.] Univ Reading, Sch Human & Environm Sci, Reading RG6 6AB, Berks, England. [Coleman, Max L.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Gazdzicka, Elzbieta] Panstwowy Inst Geol, PL-00975 Warsaw, Poland. [Semil, Julia] Univ Warsaw, Wydzial Geol, PL-02089 Warsaw, Poland. [Gatt, Peter] Univ Malta, Dept Civil Engn, Msida, Malta. RP Gruszczynski, M (reprint author), Uniwersytet Jana Kochanowskiego, Inst Geog, Swietokrzyska 15, PL-25406 Kielce, Poland. EM beerbear@onet.eu RI Coleman, Max/A-1303-2007 OI Coleman, Max/0000-0002-5514-1826 NR 75 TC 9 Z9 10 U1 0 U2 12 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0031-0182 J9 PALAEOGEOGR PALAEOCL JI Paleogeogr. Paleoclimatol. Paleoecol. PD DEC 15 PY 2008 VL 270 IS 3-4 BP 239 EP 251 DI 10.1016/j.palaeo.2008.01.035 PG 13 WC Geography, Physical; Geosciences, Multidisciplinary; Paleontology SC Physical Geography; Geology; Paleontology GA 386AE UT WOS:000261853900004 ER PT J AU Brown, CA Huot, Y Werdell, PJ Gentili, B Claustre, H AF Brown, Catherine A. Huot, Yannick Werdell, P. Jeremy Gentili, Bernard Claustre, Herve TI The origin and global distribution of second order variability in satellite ocean color and its potential applications to algorithm development SO REMOTE SENSING OF ENVIRONMENT LA English DT Article DE Remote sensing; MODIS; Optical properties; Backscattering; CDOM; Ocean color; Bio-optics ID INHERENT OPTICAL-PROPERTIES; ANTARCTIC PENINSULA WATERS; CASE-I WATERS; CASE-1 WATERS; BIOOPTICAL PROPERTIES; CHLOROPHYLL-A; PHYTOPLANKTON PIGMENTS; MULTISENSOR APPROACH; REFLECTANCE MODEL; COASTAL WATERS AB Empirical algorithms based on first order relationships between ocean color and the chlorophyll concentration ([ChI]; mg m(-3)) are widely used, but cannot explain the statistical dispersion or "anomalies" around the mean trends. We use an empirical approach that removes the first order effects of [ChI] from satellite ocean color, thus allowing us to quantify the impact on the ocean color signal of optical anomalies that vary independently of the global mean trends with remotely sensed [ChI]. We then present statistical and modeling analyses to interpret the observed anomalies in terms of their optical sources (i.e. absorption and backscattering coefficients). We identify two main sources of second order variability for a given [ChI]: 1) the amount of non-algal absorption, especially due to colored dissolved organic matter; and 2) the amplitude of the backscattering coefficient of particles. The global distribution of the anomalies displays significant regional and seasonal trends, providing important information for characterizing the marine optical environment and for inferring biogeochemical influences. We subsequently use our empirically determined anomalies to estimate the backscattering coefficient of particles and the combined absorption coefficient for colored detrital and dissolved materials. This purely empirical approach provides an independent assessment of second order optical variability for comparison with existing methods that are generally based on semi-analytical models. (C) 2008 Elsevier Inc. All rights reserved. C1 [Brown, Catherine A.; Huot, Yannick; Gentili, Bernard; Claustre, Herve] CNRS, UMR 7093, Oceanog Lab, F-06230 Villefranche Sur Mer, France. [Brown, Catherine A.; Huot, Yannick; Gentili, Bernard; Claustre, Herve] Univ Paris 06, UMR 7093, Oceanog Lab, F-06230 Villefranche Sur Mer, France. [Werdell, P. Jeremy] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Brown, CA (reprint author), CNRS, UMR 7093, Oceanog Lab, F-06230 Villefranche Sur Mer, France. EM brown@obs-vlfr.fr RI Werdell, Jeremy/D-8265-2012; Huot, Yannick/B-4497-2008; CLAUSTRE, Herve/E-6877-2011 OI Huot, Yannick/0000-0003-1793-761X; CLAUSTRE, Herve/0000-0001-6243-0258 NR 64 TC 47 Z9 48 U1 1 U2 13 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 DEC 15 PY 2008 VL 112 IS 12 BP 4186 EP 4203 DI 10.1016/j.rse.2008.06.008 PG 18 WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic Technology SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science & Photographic Technology GA 373AD UT WOS:000260942500002 ER PT J AU Bindschadler, R Vornberger, P Fleming, A Fox, A Mullins, J Binnie, D Paulsen, SJ Granneman, B Gorodetzky, D AF Bindschadler, Robert Vornberger, Patricia Fleming, Andrew Fox, Adrian Mullins, Jerry Binnie, Douglas Paulsen, Sara Jean Granneman, Brian Gorodetzky, David TI The Landsat Image Mosaic of Antarctica SO REMOTE SENSING OF ENVIRONMENT LA English DT Article DE Landsat; Antarctica; Ice sheet ID BIDIRECTIONAL REFLECTANCE; SNOW AB The Landsat Image Mosaic of Antarctica (LIMA) is the first true-color, high-spatial-resolution image of the seventh continent. It is constructed from nearly 1100 individually selected Landsat-7 ETM+ scenes. Each image was orthorectified and adjusted for geometric, sensor and illumination variations to a standardized, almost seamless surface reflectance product. Mosaicing to avoid clouds produced a high quality, nearly cloud-free benchmark data set of Antarctica for the International Polar Year from images collected primarily during 1999-2003. Multiple color composites and enhancements were generated to illustrate additional characteristics of the multispectral data including: the true appearance of the surface: discrimination between snow and bare ice; reflectance variations within bright snow; recovered reflectance values in regions of sensor saturation; and subtle topographic variations associated with ice flow. LIMA is viewable and individual scenes or user defined portions of the mosaic are downloadable at http://Iima.usgs.gov. Educational materials associated with LIMA are available at http://Iima.nasa.gov. Published by Elsevier Inc. C1 [Bindschadler, Robert] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Fleming, Andrew; Fox, Adrian] British Antarctic Survey, Cambridge, England. RP Bindschadler, R (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. EM Robert.A.Bindschadler@nasa.gov FU National Science Foundation [0541544, 0233246H]; British Antarctic Survey FX This project was supported by the National Science Foundation through grants #0541544 to NASA and #0233246H to USGS and by the British Antarctic Survey. It is regarded as a major benchmark data set of the International Polar Year. NR 8 TC 70 Z9 72 U1 1 U2 12 PU ELSEVIER SCIENCE INC PI NEW YORK PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA SN 0034-4257 J9 REMOTE SENS ENVIRON JI Remote Sens. Environ. PD DEC 15 PY 2008 VL 112 IS 12 BP 4214 EP 4226 DI 10.1016/j.rse.2008.07.006 PG 13 WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic Technology SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science & Photographic Technology GA 373AD UT WOS:000260942500004 ER PT J AU Ganguly, S Samanta, A Schull, MA Shabanov, NV Milesi, C Nemani, RR Knyazikhin, Y Myneni, RB AF Ganguly, Sangram Samanta, Arindam Schull, Mitchell A. Shabanov, Nikolay V. Milesi, Cristina Nemani, Ramakrishna R. Knyazikhin, Yuri Myneni, Ranga B. TI Generating vegetation leaf area index Earth system data record from multiple sensors. Part 2: Implementation, analysis and validation SO REMOTE SENSING OF ENVIRONMENT LA English DT Article DE Leaf area index; Validation; Accuracy; Climate data; Long term data record; AVHRR LAI; MODIS LAI; CYCLOPES; Spectral invariants; Recollision probability; Radiative transfer; Scaling; Single scattering albedo; Data uncertainties ID CYCLOPES GLOBAL PRODUCTS; LAND-SURFACE; PHOTOSYNTHETIC TRENDS; SPOT-VEGETATION; SATELLITE DATA; AFRICAN SAHEL; WHITE SPRUCE; LAI PRODUCTS; NDVI DATA; MODIS AB The evaluation of a new global monthly leaf area index (LAI) data set for the period July 1981 to December 2006 derived from AVHRR Normalized Difference Vegetation Index (NDVI) data is described. The physically based algorithm is detailed in the first of the two part series. Here, the implementation, production and evaluation of the data set are described. The data set is evaluated both by direct comparisons to ground data and indirectly through inter-comparisons with similar data sets. This indirect validation showed satisfactory agreement with existing LAI products, importantly MODIS, at a range of spatial scales, and significant correlations with key climate variables in areas where temperature and precipitation limit plant growth. The data set successfully reproduced well-documented spatio-temporal trends and inter-annual variations in vegetation activity in the northern latitudes and semi-arid tropics. Comparison with plot scale field measurements over homogeneous vegetation patches indicated a 7% underestimation when all major vegetation types are taken into account. The error in mean values obtained from distributions of AVHRR LAI and high-resolution field LAI maps for different biomes is within 0.5 LAI for six out of the ten selected sites. These validation exercises though limited by the amount of field data, and thus less than comprehensive, indicated satisfactory agreement between the LAI product and field measurements. Overall, the inter-comparison with short-term LAI data sets, evaluation of long term trends with known variations in climate variables, and validation with field measurements together build confidence in the utility of this new 26 year LAI record for long term vegetation monitoring and modeling studies. (C) 2008 Elsevier Inc. All rights reserved. C1 [Ganguly, Sangram; Samanta, Arindam; Schull, Mitchell A.; Knyazikhin, Yuri; Myneni, Ranga B.] Boston Univ, Dept Geog & Environm, Boston, MA 02215 USA. [Shabanov, Nikolay V.] NOAA NEDIS, Camp Springs, MD 20746 USA. [Milesi, Cristina; Nemani, Ramakrishna R.] NASA, Ames Res Ctr, Ecosyst Sci & Technol Branch, Moffett Field, CA 94035 USA. RP Ganguly, S (reprint author), Boston Univ, Dept Geog & Environm, 675 Commonwealth Ave, Boston, MA 02215 USA. EM sganguly@bu.edu RI Schull, Mitch/D-1663-2010; Samanta, Arindam/B-9550-2009; Myneni, Ranga/F-5129-2012 FU NASA Earth Science Enterprise FX This research was funded by NASA Earth Science Enterprise. We thank Dr. C. J. Tucker of NASA GSFC for making the GIMMS NDVI data available. NR 64 TC 52 Z9 60 U1 2 U2 33 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 DEC 15 PY 2008 VL 112 IS 12 BP 4318 EP 4332 DI 10.1016/j.rse.2008.07.013 PG 15 WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic Technology SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science & Photographic Technology GA 373AD UT WOS:000260942500011 ER PT J AU Ganguly, S Schull, MA Samanta, A Shabanov, NV Milesi, C Nemani, RR Knyazikhin, Y Myneni, RB AF Ganguly, Sangram Schull, Mitchell A. Samanta, Arindam Shabanov, Nikolay V. Milesi, Cristina Nemani, Ramakrishna R. Knyazikhin, Yuri Myneni, Ranga B. TI Generating vegetation leaf area index earth system data record from multiple sensors. Part 1: Theory SO REMOTE SENSING OF ENVIRONMENT LA English DT Article DE Leaf area index; Spectral invariant; Recollision probability; Radiative transfer; Long-term data record; AVHRR; MODIS; Scaling; Single scattering albedo; Data uncertainties ID SPECTRAL INVARIANTS; RADIATIVE-TRANSFER; SATELLITE DATA; MODIS DATA; NDVI DATA; CANOPY; ALGORITHM; MODEL; LAI; PARAMETERIZATION AB The generation of multi-decade long Earth System Data Records (ESDRs) of Leaf Area Index (LAI) and Fraction of Photosynthetically Active Radiation absorbed by vegetation (FPAR) from remote sensing measurements of multiple sensors is key to monitoring long-term changes in vegetation due to natural and anthropogenic influences. Challenges in developing such ESDRs include problems in remote sensing science (modeling of variability in global vegetation, scaling, atmospheric correction) and sensor hardware (differences in spatial resolution, spectral bands, calibration, and information content). In this paper, we develop a physically based approach for deriving LAI and FPAR products from the Advanced Very High Resolution Radiometer (AVHRR) data that are of comparable quality to the Moderate resolution Imaging Spectroradiometer (MODIS) LAI and FPAR products, thus realizing the objective of producing a long (multi-decadal) time series of these products. The approach is based on the radiative transfer theory of canopy spectral invariants which facilitates parameterization of the canopy spectral bidirectional reflectance factor (BRF). The methodology permits decoupling of the structural and radiometric components and obeys the energy conservation law. The approach is applicable to any optical sensor, however, it requires selection of sensor-specific values of configurable parameters, namely, the single scattering albedo and data uncertainty. According to the theory of spectral invariants, the single scattering albedo is a function of the spatial scale, and thus, accounts for the variation in BRF with sensor spatial resolution. Likewise, the single scattering albedo accounts for the variation in spectral BRF with sensor bandwidths. The second adjustable parameter is data uncertainty. which accounts for varying information content of the remote sensing measurements, i.e., Normalized Difference Vegetation Index (NDVI, low information content), vs. spectral BRF (higher information content). Implementation of this approach indicates good consistency in LAI values retrieved from NDVI (AVHRR-mode) and spectral BRF (MODIS-mode). Specific details of the implementation and evaluation of the derived products are detailed in the second part of this two-paper series. (C) 2008 Elsevier Inc. All rights reserved. C1 [Ganguly, Sangram; Schull, Mitchell A.; Samanta, Arindam; Knyazikhin, Yuri; Myneni, Ranga B.] Boston Univ, Dept Geog & Environm, Boston, MA 02215 USA. [Shabanov, Nikolay V.] NOAA NESDIS, Camp Springs, MD 20746 USA. [Milesi, Cristina; Nemani, Ramakrishna R.] NASA, Ames Res Ctr, Ecosyst Sci & Technol Branch, Moffett Field, CA 94035 USA. RP Ganguly, S (reprint author), Boston Univ, Dept Geog & Environm, 675 Commonwealth Ave, Boston, MA 02215 USA. EM sganguly@bu.edu RI Schull, Mitch/D-1663-2010; Samanta, Arindam/B-9550-2009; ganguly, sangram/B-5108-2010; Myneni, Ranga/F-5129-2012 FU NASA Earth Science Enterprise FX This research was funded by NASA Earth Science Enterprise. We thank Dr. C. J. Tucker of NASA GSFC for making the GIMMS NDVI data available. NR 50 TC 67 Z9 75 U1 1 U2 28 PU ELSEVIER SCIENCE INC PI NEW YORK PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA SN 0034-4257 J9 REMOTE SENS ENVIRON JI Remote Sens. Environ. PD DEC 15 PY 2008 VL 112 IS 12 BP 4333 EP 4343 DI 10.1016/j.rse.2008.07.014 PG 11 WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic Technology SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science & Photographic Technology GA 373AD UT WOS:000260942500012 ER PT J AU Li, LM Gierasch, PJ Achterberg, RK Conrath, BJ Flasar, FM Vasavada, AR Ingersoll, AP Banfield, D Simon-Miller, AA Fletcher, LN AF Li Liming Gierasch, Peter J. Achterberg, Richard K. Conrath, Barney J. Flasar, F. Michael Vasavada, Ashwin R. Ingersoll, Andrew P. Banfield, Don Simon-Miller, Amy A. Fletcher, Leigh N. TI Strong jet and a new thermal wave in Saturn's equatorial stratosphere SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID QUASI-BIENNIAL OSCILLATION; CLOUD LEVEL; UPPER TROPOSPHERE; ROTATION PERIOD; ATMOSPHERE; JUPITER; TEMPERATURES; SYSTEM; SPOTS; FIELD AB The strong jet, with a speed between 500 and 600 m/s, is inferred in the equatorial region of Saturn by combining the nadir and limb observations of Composite Infrared Spectrometer (CIRS) aboard the Cassini spacecraft. A similar jet was discovered on Jupiter (F. M. Flasar et al., 2004a). These discoveries raise the possibility that intense jets are common in the equatorial stratospheres of giant planets. An equatorial wave with wavenumber similar to 9 is revealed in the stratosphere of Saturn by the CIRS high spatial-resolution thermal maps. Our discussion based on the phase velocity suggests that the equatorial wave is probably a Rossby-gravity wave. The discovery of an equatorial wave in the stratosphere suggests that Saturn's equatorial oscillations (T. Fouchet et al., 2008; G. S. Orton et al., 2008) may be driven by vertically propagating waves, the same mechanism that drives the quasi-biennial oscillation (QBO) on Earth. C1 [Li Liming; Gierasch, Peter J.; Conrath, Barney J.; Banfield, Don] Cornell Univ, Dept Astron, Ithaca, NY 14853 USA. [Achterberg, Richard K.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Flasar, F. Michael; Simon-Miller, Amy A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Vasavada, Ashwin R.; Fletcher, Leigh N.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Ingersoll, Andrew P.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. RP Li, LM (reprint author), Cornell Univ, Dept Astron, Ithaca, NY 14853 USA. EM liming@astro.cornell.edu RI Fletcher, Leigh/D-6093-2011; Flasar, F Michael/C-8509-2012; Simon, Amy/C-8020-2012; OI Fletcher, Leigh/0000-0001-5834-9588; Simon, Amy/0000-0003-4641-6186; Banfield, Don/0000-0003-2664-0164 NR 31 TC 5 Z9 5 U1 0 U2 5 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD DEC 13 PY 2008 VL 35 IS 23 AR L23208 DI 10.1029/2008GL035515 PG 5 WC Geosciences, Multidisciplinary SC Geology GA 383JG UT WOS:000261669300002 ER PT J AU Lau, KM Zhou, YP Wu, HT AF Lau, K. -M. Zhou, Y. P. Wu, H. -T. TI Have tropical cyclones been feeding more extreme rainfall? SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID WESTERN NORTH PACIFIC; ATLANTIC HURRICANE SEASON; GLOBAL CLIMATE-CHANGE; UNITED-STATES; INTERANNUAL VARIABILITY; CLIMATOLOGICAL RAINFALL; SURFACE TEMPERATURE; STRONG ASSOCIATION; AFRICAN RAINFALL; EL-NINO AB We have conducted a study of the relationship between tropical cyclone (TC) and extreme rain events using GPCP and TRMM rainfall data, and storm track data for July through November (JASON) in the North Atlantic (NAT) and the western North Pacific (WNP). Extreme rain events are defined in terms of percentile rainrate, and TC-rain by rainfall associated with a named TC. Results show that climatologically, 8% of rain events and 17% of the total rain amount in NAT are accounted by TCs, compared to 9% of rain events, and 21% of rain amount in WNP. The fractional contribution of accumulated TC-rain to total rain, Omega, increases nearly linearly as a function of rainrate. Extending the analyses using GPCP pentad data for 1979-2005, and for the post-SSM/I period (1988-2005), we find that while there is no significant trend in the total JASON rainfall over NAT or WNP, there is a positive significant trend in heavy rain over both basins for the 1979-2005 period, but not for the post-SSM/I period. Trend analyses of Omega for both periods indicate that TCs have been feeding increasingly more to rainfall extremes in NAT, where the expansion of the warm pool area can explain slightly more than 50% of the change in observed trend in total TC rainfall. In WNP, trend signals for Omega are mixed, and the long-term relationship between TC rain and warm pool area is strongly influenced by interannual and interdecadal variability. C1 [Lau, K. -M.] NASA, Goddard Space Flight Ctr, Atmospheres Lab, Greenbelt, MD 20771 USA. [Zhou, Y. P.] Univ Maryland Baltimore Cty, Goddard Earth Sci & Technol Ctr, Catonsville, MD USA. [Wu, H. -T.] Sci Syst & Applicat Inc, Lanham, MD USA. RP Lau, KM (reprint author), NASA, Goddard Space Flight Ctr, Atmospheres Lab, Code 613, Greenbelt, MD 20771 USA. EM william.k.lau@nasa.gov; yaping.zhou-1@nasa.gov; hueytzu.wu-1@mail.nasa.gov RI Lau, William /E-1510-2012 OI Lau, William /0000-0002-3587-3691 FU Precipitation Measuring Mission, NASA Earth Science Division FX This work is supported by the Precipitation Measuring Mission (Headquarter Manager: Dr. R. Kakar), NASA Earth Science Division. We thank Dr. Chris Landsea and two anonymous reviewers for constructive comments that have improved the manuscript. NR 54 TC 32 Z9 32 U1 0 U2 4 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 DEC 13 PY 2008 VL 113 IS D23 AR D23113 DI 10.1029/2008JD009963 PG 12 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 383KE UT WOS:000261671700002 ER PT J AU Matsoukas, C Banks, AC Pavlakis, KG Hatzianastassiou, N Stackhouse, PW Vardavas, I AF Matsoukas, C. Banks, A. C. Pavlakis, K. G. Hatzianastassiou, N. Stackhouse, P. W., Jr. Vardavas, I. TI Reply to comment by Kara and Barron on "Seasonal heat budgets of the Red and Black seas'' SO JOURNAL OF GEOPHYSICAL RESEARCH-OCEANS LA English DT Editorial Material ID GLOBAL DISTRIBUTION; RADIATION BUDGET; MODEL C1 [Matsoukas, C.] Univ Aegean, Dept Environm, GR-81100 Mitilini, Greece. [Banks, A. C.] Hellen Ctr Marine Res, GR-71003 Iraklion, Greece. [Hatzianastassiou, N.] Univ Ioannina, Dept Phys, Lab Meteorol, GR-45110 Ioannina, Greece. [Pavlakis, K. G.] Technol Educ Inst Crete, Dept Gen Appl Sci, GR-71110 Iraklion, Greece. [Stackhouse, P. W., Jr.] NASA, Langley Res Ctr, Hampton, VA 23681 USA. [Vardavas, I.] Univ Crete, Dept Phys, GR-71003 Iraklion, Greece. RP Matsoukas, C (reprint author), Univ Aegean, Dept Environm, Xenia Bldg,Univ Hill, GR-81100 Mitilini, Greece. EM matsoukas@aegean.gr RI Vardavas, Ilias/G-7310-2011 NR 13 TC 0 Z9 0 U1 0 U2 1 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9275 J9 J GEOPHYS RES-OCEANS JI J. Geophys. Res.-Oceans PD DEC 13 PY 2008 VL 113 IS C12 AR C12009 DI 10.1029/2008JC004917 PG 3 WC Oceanography SC Oceanography GA 383KX UT WOS:000261673600004 ER PT J AU Hong, G Yang, P Minnis, P Hu, YX North, G AF Hong, Gang Yang, Ping Minnis, Patrick Hu, Yong X. North, Gerald TI Do contrails significantly reduce daily temperature range? SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID UNITED-STATES; CLIMATE; CIRRUS; WEATHER; CLOUDS; TRENDS; IMPACT; CLEAR AB One of the most visible anthropogenic phenomena in the atmosphere is the occurrence of contrails. The direct effects of contrails on surface temperature are investigated on the basis of the data sets for the cloud cover and surface temperature over the conterminous United States for the period 1971-2001. It is shown that the increase of the average daily temperature range (DTR) over the United States during the three-day grounding period of 11-14 September 2001 cannot be attributed to the absence of contrails, a subject was debated in several previous studies. The present analysis suggests that the DTR is attributed to the change of low cloudiness. Citation: Hong, G., P. Yang, P. Minnis, Y. X. Hu, and G. North (2008), Do contrails significantly reduce daily temperature range?, Geophys. Res. Lett., 35, L23815, doi:10.1029/2008GL036108. C1 [Hong, Gang; Yang, Ping; North, Gerald] Texas A&M Univ, Dept Atmospher Sci, College Stn, TX 77843 USA. [Minnis, Patrick; Hu, Yong X.] NASA, Langley Res Ctr, Hampton, VA 23681 USA. RP Hong, G (reprint author), Texas A&M Univ, Dept Atmospher Sci, College Stn, TX 77843 USA. EM hong@ariel.met.tamu.edu RI Minnis, Patrick/G-1902-2010; Yang, Ping/B-4590-2011; North, Gerald/G-1019-2011; Hong, Gang/A-2323-2012; Hu, Yongxiang/K-4426-2012 OI Minnis, Patrick/0000-0002-4733-6148; FU U.S.Department of Transportation; Volpe National Transportation System Center [DTRT57-08-C-10005]; National Science Foundation [ATM-0239605] FX This study is partly supported by U.S.Department of Transportation (DOT) Volpe National Transportation System Center under contract DTRT57-08-C-10005 managed by Mohan Gupta and the National Science Foundation under ATM-0239605 managed by Bradley Smull. ECMWF ERA-40 data used in this study/project have been provided by ECMWF/ have been obtained from the ECMWF Data Server. The ISCCP D1 data were obtained from the International Satellite Cloud Climatology Project web site http:// isccp.giss.nasa.gov maintained by the ISCCP research group at the NASA Goddard Institute for Space Studies, New York, NY on January, 2005. Data set 3200 (DSI-3200) was obtained from National Climatic Data Center, Asheville, NC. G. Hong gratefully thanks W. Spangler at NCAR/CISL/DSS for accessing the data set DSI3200. We also thank the two reviewers for their constructive comments. NR 17 TC 6 Z9 8 U1 1 U2 5 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD DEC 12 PY 2008 VL 35 IS 23 AR L23815 DI 10.1029/2008GL036108 PG 4 WC Geosciences, Multidisciplinary SC Geology GA 383JD UT WOS:000261669000004 ER PT J AU Briggs, RW Sieh, K Amidon, WH Galetzka, J Prayudi, D Suprihanto, I Sastra, N Suwargadi, B Natawidjaja, D Farr, TG AF Briggs, Richard W. Sieh, Kerry Amidon, William H. Galetzka, John Prayudi, Dudi Suprihanto, Imam Sastra, Nugraha Suwargadi, Bambang Natawidjaja, Danny Farr, Thomas G. TI Persistent elastic behavior above a megathrust rupture patch: Nias island, West Sumatra SO JOURNAL OF GEOPHYSICAL RESEARCH-SOLID EARTH LA English DT Article ID CASCADIA SUBDUCTION ZONE; SEA-LEVEL CHANGES; 1964 ALASKA EARTHQUAKE; MALAY-THAI PENINSULA; SIMEULUE EARTHQUAKE; CRUSTAL DEFORMATION; SOUTHWEST JAPAN; COASTAL DEFORMATION; ANDAMAN EARTHQUAKE; TECTONIC MOVEMENTS AB We quantify fore-arc deformation using fossil reefs to test the assumption commonly made in seismic cycle models that anelastic deformation of the fore arc is negligible. Elevated coral microatolls, paleoreef flats, and chenier plains show that the Sumatran outer arc island of Nias has experienced a complex pattern of relatively slow long-term uplift and subsidence during the Holocene epoch. This same island rose up to 2.9 m during the M-w 8.7 Sunda megathrust rupture in 2005. The mismatch between the 2005 and Holocene uplift patterns, along with the overall low rates of Holocene deformation, reflects the dominance of elastic strain accumulation and release along this section of the Sunda outer arc high and the relatively subordinate role of upper plate deformation in accommodating long-term plate convergence. The fraction of 2005 uplift that will be retained permanently is generally <4% for sites that experienced more than 0.25 m of coseismic uplift. Average uplift rates since the mid-Holocene range from 1.5 to -0.2 mm/a and are highest on the eastern coast of Nias, where coseismic uplift was nearly zero in 2005. The pattern of long-term uplift and subsidence is consistent with slow deformation of Nias along closely spaced folds in the north and trenchward dipping back thrusts in the southeast. Low Holocene tectonic uplift rates provide for excellent geomorphic and stratigraphic preservation of the mid-Holocene relative sea level high, which was under way by similar to 7.3 ka and persisted until similar to 2 ka. C1 [Briggs, Richard W.; Sieh, Kerry; Amidon, William H.; Galetzka, John] CALTECH, Div Geol & Planetary Sci, Tecton Observ, Pasadena, CA 91125 USA. [Farr, Thomas G.] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. [Prayudi, Dudi; Sastra, Nugraha; Suwargadi, Bambang; Natawidjaja, Danny] Indonesian Inst Sci, Res Ctr Geotechnol, Bandung 40135, Indonesia. RP Briggs, RW (reprint author), US Geol Survey, Geol Hazards Team, MS 966,Box 25046, Golden, CO 80225 USA. EM rbriggs@usgs.gov RI Briggs, Richard/A-1348-2013; OI Briggs, Richard/0000-0001-8108-0046; Farr, Thomas/0000-0001-5406-2096 FU NSF [EAR-0610078]; Gordon and Betty Moore Foundation FX We thank the Captain and crew of the Mentawai Indah. Thanks to Hong-Wei Chiang and Larry Edwards for the U-Th dates. Dick Peltier and Rosemarie Drummond kindly provided predictions from the ICE-5G (VM2) model, and Aron Meltzner generously provided tide model calculations. We benefited greatly from discussions with Mike Gagan, Jean-Philippe Avouac, Glenn Milne, Chris Goldfinger, Harvey Kelsey, Ben Horton, and Heidrun Kopp. We also thank Daniel Melnick, Alan Nelson, two anonymous reviewers, and Associate Editor Greg Moore for their reviews and discussion of our manuscript. This work was supported by NSF (EAR-0610078) and a grant from the Gordon and Betty Moore Foundation. This is Caltech Tectonics Observatory contribution 80. NR 94 TC 19 Z9 19 U1 0 U2 5 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 DEC 12 PY 2008 VL 113 IS B12 AR B12406 DI 10.1029/2008JB005684 PG 28 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 383QK UT WOS:000261688200001 ER PT J AU Wilson, JW Ott, CM Quick, L Davis, R Bentrup, KHZ Crabbe, A Richter, E Sarker, S Barrila, J Porwollik, S Cheng, P McClelland, M Tsaprailis, G Radabaugh, T Hunt, A Shah, M Nelman-Gonzalez, M Hing, S Parra, M Dumars, P Norwood, K Bober, R Devich, J Ruggles, A CdeBaca, A Narayan, S Benjamin, J Goulart, C Rupert, M Catella, L Schurr, MJ Buchanan, K Morici, L McCracken, J Porter, MD Pierson, DL Smith, SM Mergeay, M Leys, N Stefanyshyn-Piper, HM Gorie, D Nickerson, CA AF Wilson, James W. Ott, C. Mark Quick, Laura Davis, Richard Bentrup, Kerstin Hoener zu Crabbe, Aurelie Richter, Emily Sarker, Shameema Barrila, Jennifer Porwollik, Steffen Cheng, Pui McClelland, Michael Tsaprailis, George Radabaugh, Timothy Hunt, Andrea Shah, Miti Nelman-Gonzalez, Mayra Hing, Steve Parra, Macarena Dumars, Paula Norwood, Kelly Bober, Ramona Devich, Jennifer Ruggles, Ashleigh CdeBaca, Autumn Narayan, Satro Benjamin, Joseph Goulart, Carla Rupert, Mark Catella, Luke Schurr, Michael J. Buchanan, Kent Morici, Lisa McCracken, James Porter, Marc D. Pierson, Duane L. Smith, Scott M. Mergeay, Max Leys, Natalie Stefanyshyn-Piper, Heidemarie M. Gorie, Dominic Nickerson, Cheryl A. TI Media Ion Composition Controls Regulatory and Virulence Response of Salmonella in Spaceflight SO PLOS ONE LA English DT Article AB The spaceflight environment is relevant to conditions encountered by pathogens during the course of infection and induces novel changes in microbial pathogenesis not observed using conventional methods. It is unclear how microbial cells sense spaceflight-associated changes to their growth environment and orchestrate corresponding changes in molecular and physiological phenotypes relevant to the infection process. Here we report that spaceflight-induced increases in Salmonella virulence are regulated by media ion composition, and that phosphate ion is sufficient to alter related pathogenesis responses in a spaceflight analogue model. Using whole genome microarray and proteomic analyses from two independent Space Shuttle missions, we identified evolutionarily conserved molecular pathways in Salmonella that respond to spaceflight under all media compositions tested. Identification of conserved regulatory paradigms opens new avenues to control microbial responses during the infection process and holds promise to provide an improved understanding of human health and disease on Earth. C1 [Quick, Laura; Davis, Richard; Crabbe, Aurelie; Richter, Emily; Sarker, Shameema; Barrila, Jennifer; Nickerson, Cheryl A.] Arizona State Univ, Ctr Infect Dis & Vaccinol, Biodesign Inst, Tempe, AZ 85287 USA. [Wilson, James W.; Quick, Laura] Villanova Univ, Dept Biol, Villanova, PA 19085 USA. [Ott, C. Mark; Pierson, Duane L.] NASA, Johnson Space Center, Habitabil & Environm Factors Div, Houston, TX USA. [Bentrup, Kerstin Hoener zu; Morici, Lisa] Tulane Univ, Hlth Sci Ctr, New Orleans, LA 70118 USA. [Crabbe, Aurelie] Free Univ Brussels, Flanders Inst Biotechnol, B-1050 Brussels, Belgium. [Crabbe, Aurelie; Mergeay, Max; Leys, Natalie] Belgian Nuclear Res Ctr, Mol, Belgium. [Porwollik, Steffen; Cheng, Pui; McClelland, Michael] Sidney Kimmel Canc Ctr, San Diego, CA USA. [Tsaprailis, George; Radabaugh, Timothy; Hunt, Andrea] Univ Arizona, Ctr Toxicol, Tucson, AZ 85721 USA. [Shah, Miti] Arizona State Univ, Ctr Glycosci Technol, Biodesign Inst, Tempe, AZ 85287 USA. [Nelman-Gonzalez, Mayra] Wyle Lab, Houston, TX USA. [Hing, Steve; Parra, Macarena; Dumars, Paula] NASA, Ames Res Ctr, Moffett Field, CA USA. [Norwood, Kelly; Bober, Ramona; Devich, Jennifer; Ruggles, Ashleigh; CdeBaca, Autumn; Narayan, Satro; Benjamin, Joseph; Catella, Luke] Kennedy Space Ctr, Space Life Sci Lab, Cape Canaveral, FL USA. [Goulart, Carla; Rupert, Mark] Univ Colorado, Boulder, CO 80309 USA. [Schurr, Michael J.] Univ Colorado, Sch Med, Aurora, CO USA. [Buchanan, Kent] Oklahoma City Univ, Oklahoma City, OK USA. [McCracken, James] Univ Chicago, Sect Gen Surg, Chicago, IL 60637 USA. [Porter, Marc D.] Univ Utah, Dept Chem, Chem Engn & Bioengn, Salt Lake City, UT 84112 USA. [Smith, Scott M.] Natl Aeronaut & Space Adm, Johnson Space Ctr, Human Adapt & Countermeasures Div, Houston, TX USA. [Stefanyshyn-Piper, Heidemarie M.; Gorie, Dominic] NASA, Johnson Space Ctr, Astronaut Office, Houston, TX USA. RP Wilson, JW (reprint author), Arizona State Univ, Ctr Infect Dis & Vaccinol, Biodesign Inst, Tempe, AZ 85287 USA. EM Cheryl.A.Nickerson@asu.edu RI McClelland, Michael/A-8583-2011; Mergeay, Max/H-2003-2011; OI McClelland, Michael/0000-0003-1788-9347 FU NASA [NCC2-1362]; NIEHS [ES06694]; NIH/NCI [CA023074]; BIO5 Institute of the University of Arizona; King Baudouin Foundation [Henri Benedictus Fellowship]; Belgian American Educational Foundation FX This work was supported by NASA grant NCC2-1362 to CAN; Arizona Proteomics Consortium supported by NIEHS grant ES06694 to the SWEHSC, NIH/NCI grant CA023074 to the AZCC, and by the BIO5 Institute of the University of Arizona; AC supported by Henri Benedictus Fellowship of the King Baudouin Foundation and the Belgian American Educational Foundation (B.A.E.F.). The funders had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript. NR 33 TC 47 Z9 53 U1 0 U2 20 PU PUBLIC LIBRARY SCIENCE PI SAN FRANCISCO PA 185 BERRY ST, STE 1300, SAN FRANCISCO, CA 94107 USA SN 1932-6203 J9 PLOS ONE JI PLoS One PD DEC 12 PY 2008 VL 3 IS 12 AR e3923 DI 10.1371/journal.pone.0003923 PG 10 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 436ZW UT WOS:000265456300003 PM 19079590 ER PT J AU Huang, J Minnis, P Chen, B Huang, ZW Liu, ZY Zhao, QY Yi, YH Ayers, JK AF Huang, Jianping Minnis, Patrick Chen, Bin Huang, Zhongwei Liu, Zhaoyan Zhao, Qingyun Yi, Yuhong Ayers, J. Kirk TI Long-range transport and vertical structure of Asian dust from CALIPSO and surface measurements during PACDEX SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID APRIL 1998; LIDAR OBSERVATIONS; LOESS PLATEAU; MINERAL DUST; SAHARAN DUST; EAST-ASIA; AEROSOLS; CLIMATE; NETWORK; EVENTS AB Knowledge of long-range transport and vertical distribution of Asian dust aerosols in the free troposphere is important for estimating their impact on climate. Cloud-Aerosol Lidar and Infrared Pathfinder Satellite Observations (CALIPSO), surface micropulse lidar (MPL), and standard surface measurements are used to directly observe the long-range transport and vertical distribution of Asian dust aerosols in the free troposphere during the Pacific Dust Experiment (PACDEX). The MPL measurements were made at the Loess Plateau (35.95 degrees N, 104.1 degrees E) near the major dust source regions of the Taklamakan and Gobi deserts. Dust events are more frequent in the Taklamakan, where floating dust dominates, while more intensive, less frequent dust storms are more common in the Gobi region. The vertical distribution of the CALIPSO backscattering/depolarization ratios indicate that nonspherically shaped dust aerosols floated from near the ground to an altitude of approximately 9 km around the source regions. This suggests the possible long-range transport of entrained dust aerosols via upper tropospheric westerly jets. A very distinct large depolarization layer was also identified between 8 and 10 km over eastern China and the western Pacific Ocean corresponding to dust aerosols transported from the Taklamakan and Gobi areas, as confirmed by back trajectory analyses. The combination of these dust sources results in a two-layer or multilayered dust structure over eastern China and the western Pacific Ocean. C1 [Huang, Jianping; Chen, Bin; Huang, Zhongwei] Lanzhou Univ, Coll Atmospher Sci, Lanzhou 730000, Peoples R China. [Yi, Yuhong; Ayers, J. Kirk] Sci Syst & Applicat Inc, Hampton, VA 23666 USA. [Liu, Zhaoyan] Natl Inst Aerosp, Hampton, VA 23666 USA. [Minnis, Patrick] NASA, Langley Res Ctr, Hampton, VA 23666 USA. [Zhao, Qingyun] Gansu Meteorol Bur, Lanzhou 730000, Peoples R China. RP Huang, J (reprint author), Lanzhou Univ, Coll Atmospher Sci, Lanzhou 730000, Peoples R China. EM hjp@lzu.edu.cn RI Liu, Zhaoyan/A-9604-2009; Liu, Zhaoyan/B-1783-2010; Minnis, Patrick/G-1902-2010; Huang, Zhongwei/K-5484-2013 OI Liu, Zhaoyan/0000-0003-4996-5738; Minnis, Patrick/0000-0002-4733-6148; FU National Science Foundation of China [40628005, 40633017]; NASA Science Mission Directorate FX This research is supported by National Science Foundation of China under grants 40628005 and 40633017 and the NASA Science Mission Directorate through the CALIPSO Project and the Radiation Sciences Program. The CALIPSO data were obtained from the NASA Langley Atmospheric Science Data Center (ASDC). NR 42 TC 123 Z9 139 U1 9 U2 29 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD DEC 11 PY 2008 VL 113 IS D23 AR D23212 DI 10.1029/2008JD010620 PG 13 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 383JQ UT WOS:000261670300003 ER PT J AU Xi, DJ Zhang, H Furst, S Chen, B Pei, QB AF Xi, Dongjuan Zhang, Han Furst, Stephen Chen, Bin Pei, Qibing TI Electrochemical Synthesis and Photovoltaic Property of Cadmium Sulfide-Polybithiophene Interdigitated Nanohybrid Thin Films SO JOURNAL OF PHYSICAL CHEMISTRY C LA English DT Article ID HYBRID SOLAR-CELLS; BULK-HETEROJUNCTION; CONJUGATED-POLYMER; POLYTHIOPHENE FILMS; MESOPOROUS TITANIA; CONTROLLED GROWTH; NANOCRYSTALS; RAMAN; NANOPARTICLES; COMPOSITES AB Interdigitated hybrid films consisting of cadmium sulfide (CdS) nanorod arrays and interpenetrating polybithiophene have been synthesized by electrochemical depositions. The vertically aligned CdS nanorods were self-assembled on gold-coated glass substrates through a simple cathodic process of an electrolyte solution containing cadmium sulfate and potassium thiocyanate, without the use of any templates. The conjugated polymer polybithiophene was deposited into the nanorod arrays by in situ electrochemical polymerization. The resulting interdigitated nanohybrid films showed dense packing of the polymer in the nanorod arrays with a filling ratio estimated to be 76%. Raman spectroscopy and Fourier transform infrared revealed charge-transfer between the polymer and the CdS nanorods, consistent with the high filling ratio and improved polymer-CdS interface. Solar cells based on these hybrid films with vapor-deposited aluminum cathode exhibited a diode characteristic with a rectification ratio of 10(3) at +/- 1 V. The measured open-circuit voltage was 0.84 V, and the short-circuit current was 0.52 mA/cm(2). The overall power conversion efficiency was 0.38%. C1 [Xi, Dongjuan; Zhang, Han; Pei, Qibing] Univ Calif Los Angeles, Dept Mat Sci & Engn, Henry Samueli Sch Engn & Appl Sci, Los Angeles, CA 90095 USA. [Furst, Stephen] N Carolina State Univ, NASA, Dept Elect Engn, Space Program, Moffett Field, CA 94035 USA. [Chen, Bin] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Pei, QB (reprint author), Univ Calif Los Angeles, Dept Mat Sci & Engn, Henry Samueli Sch Engn & Appl Sci, Los Angeles, CA 90095 USA. EM qpei@seas.ucla.edu RI Pei, Qibing/N-7497-2015 FU National Science Foundation [0507294]; Defense Threat Reduction Agency [HDTRA1-07-1-0028] FX The authors would like to thank Dr. Haizheng Zhong for valuable discussions. This work is financially supported by the National Science Foundation under Grant No. 0507294 and the Defense Threat Reduction Agency Grant No. HDTRA1-07-1-0028. NR 52 TC 19 Z9 21 U1 2 U2 18 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 DEC 11 PY 2008 VL 112 IS 49 BP 19765 EP 19769 DI 10.1021/jp807868j PG 5 WC Chemistry, Physical; Nanoscience & Nanotechnology; Materials Science, Multidisciplinary SC Chemistry; Science & Technology - Other Topics; Materials Science GA 379WJ UT WOS:000261426600085 ER PT J AU Perera, TA Chapin, EL Austermann, JE Scott, KS Wilson, GW Halpern, M Pope, A Scott, D Yun, MS Lowenthal, JD Morrison, G Aretxaga, I Bock, JJ Coppin, K Crowe, M Frey, L Hughes, DH Kang, Y Kim, S Mauskopf, PD AF Perera, T. A. Chapin, E. L. Austermann, J. E. Scott, K. S. Wilson, G. W. Halpern, M. Pope, A. Scott, D. Yun, M. S. Lowenthal, J. D. Morrison, G. Aretxaga, I. Bock, J. J. Coppin, K. Crowe, M. Frey, L. Hughes, D. H. Kang, Y. Kim, S. Mauskopf, P. D. TI An AzTEC 1.1 mm survey of the GOODS-N field - I. Maps, catalogue and source statistics SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE instrumentation: detectors; galaxies: high redshift; galaxies: starburst; submillimetre ID DEGREE EXTRAGALACTIC SURVEY; SCUBA SUPER-MAP; DEEP SUBMILLIMETER SURVEY; 1200-MU-M MAMBO SURVEY; NUMBER COUNTS; HIGH-REDSHIFT; LOCKMAN HOLE; COSMOS FIELD; GALAXIES; NORTH AB We have conducted a deep and uniform 1.1 mm survey of the Great Observatories Origins Deep Survey-North (GOODS-N) field with AzTEC on the James Clerk Maxwell Telescope. Here, we present the first results from this survey including maps, the source catalogue and 1.1 mm number counts. The results presented here were obtained from a 245 arcmin(2) region with a near uniform coverage to a depth of 0.96-1.16 mJy beam(-1). Our robust catalogue contains 28 source candidates detected with S/N >= 3.75, only similar to 1-2 of which are expected to be spurious detections. Of these source candidates, eight are also detected by Submillimetre Common-User Bolometer Array ( SCUBA) at 850 mu m in regions where there is a good overlap between the two surveys. The major advantage of our survey over that with SCUBA is the uniformity of coverage. We calculate number counts using two different techniques: the first using a frequentist parameter estimation and the second using a Bayesian method. The two sets of results are in good agreement. We find that the 1.1 mm differential number counts are well described in the 2-6 mJy range by the functional form dN/dS = N'(S'/S) exp(-S/S') with fitted parameters S' = 1.25 +/- 0.38 mJy and dN/dS = 300 +/- 90 mJy(-1) deg(-2) at 3 mJy. C1 [Perera, T. A.; Austermann, J. E.; Scott, K. S.; Wilson, G. W.; Yun, M. S.] Univ Massachusetts, Dept Astron, Amherst, MA 01003 USA. [Chapin, E. L.; Halpern, M.; Pope, A.; Scott, D.; Crowe, M.; Frey, L.] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada. [Pope, A.] Natl Opt Astron Observ, Tucson, AZ 85719 USA. [Lowenthal, J. D.] Smith Coll, Dept Astron, Northampton, MA 01063 USA. [Morrison, G.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. [Morrison, G.] Canada France Hawaii Telescope Corp, Kamuela, HI 96743 USA. [Aretxaga, I.; Hughes, D. H.] Inst Nacl Astrofis Opt & Electr, Puebla, Mexico. [Bock, J. J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Coppin, K.] Univ Durham, Inst Computat Cosmol, Durham DH1 3LE, England. [Kang, Y.; Kim, S.] Sejong Univ, Dept Astron & Space Sci, Seoul, South Korea. [Mauskopf, P. D.] Cardiff Univ, Cardiff, S Glam, Wales. RP Perera, TA (reprint author), Univ Massachusetts, Dept Astron, Amherst, MA 01003 USA. EM perera@astro.umass.edu OI Scott, Douglas/0000-0002-6878-9840 FU NSF [AST 05-40852]; Korea Science & Engineering Foundation (KOSEF); Astrophysical Research Center of the Structure and Evolution of the Cosmos (ARCSEC); CONACT [60878, 50786]; NASA through the Spitzer Space Telescope Fellowship Program; Jet Propulsion Laboratory; California Institute of Technology; Science and Technology Facilities Council; Natural Sciences and Engineering Research Council of Canada FX The authors are grateful to J. Aguirre, J. Karakla, K. Souccar, I. Coulson, R. Tilanus, R. Kackley, D. Haig, S. Doyle, and the observatory staff at the JCMT who made these observations possible. Support for this work was provided, in part, by the NSF grant AST 05-40852 and the grant from the Korea Science & Engineering Foundation (KOSEF) under a cooperative Astrophysical Research Center of the Structure and Evolution of the Cosmos (ARCSEC). DHH and IA acknowledge partial support by CONACT from research grants 60878 and 50786. AP acknowledges support provided by NASA through the Spitzer Space Telescope Fellowship Program, through a contract issued by the Jet Propulsion Laboratory, California Institute of Technology under a contract with NASA. KC acknowledges support from the Science and Technology Facilities Council. DS and MH acknowledge support from the Natural Sciences and Engineering Research Council of Canada. NR 37 TC 86 Z9 86 U1 1 U2 1 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD DEC 11 PY 2008 VL 391 IS 3 BP 1227 EP 1238 DI 10.1111/j.1365-2966.2008.13902.x PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 377QK UT WOS:000261265500016 ER PT J AU Deming, D AF Deming, Drake TI ASTROPHYSICS Quest for a habitable world SO NATURE LA English DT Editorial Material ID EXTRASOLAR PLANET; HD 189733B; WATER; ATMOSPHERE; SPECTRUM; STAR C1 NASA, Solar Syst Explorat Div, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Deming, D (reprint author), NASA, Solar Syst Explorat Div, Goddard Space Flight Ctr, Code 693, Greenbelt, MD 20771 USA. EM leo.d.deming@nasa.gov NR 11 TC 1 Z9 1 U1 0 U2 2 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 0028-0836 J9 NATURE JI Nature PD DEC 11 PY 2008 VL 456 IS 7223 BP 714 EP 715 DI 10.1038/456714a PG 2 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 381TX UT WOS:000261559900029 PM 19079042 ER PT J AU Abe, K Fuke, H Haino, S Hams, T Itazaki, A Kim, KC Kumazawa, T Lee, MH Makida, Y Matsuda, S Matsumoto, K Mitchell, JW Moiseev, AA Myers, Z Nishimura, J Nozaki, M Orito, R Ormes, JF Sasaki, M Seo, ES Shikaze, Y Streitmatter, RE Suzuki, J Takasugi, Y Takeuchi, K Tanaka, K Yamagami, T Yamamoto, A Yoshida, T Yoshimura, K AF Abe, K. Fuke, H. Haino, S. Hams, T. Itazaki, A. Kim, K. C. Kumazawa, T. Lee, M. H. Makida, Y. Matsuda, S. Matsumoto, K. Mitchell, J. W. Moiseev, A. A. Myers, Z. Nishimura, J. Nozaki, M. Orito, R. Ormes, J. F. Sasaki, M. Seo, E. S. Shikaze, Y. Streitmatter, R. E. Suzuki, J. Takasugi, Y. Takeuchi, K. Tanaka, K. Yamagami, T. Yamamoto, A. Yoshida, T. Yoshimura, K. TI Measurement of the cosmic-ray low-energy antiproton spectrum with the first BESS-Polar Antarctic flight SO PHYSICS LETTERS B LA English DT Article DE Cosmic-ray antiproton; Solar modulation; Superconducting spectrometer ID SECONDARY ANTIPROTONS; PARTICLE ASTROPHYSICS; SOLAR MINIMUM; CURRENT SHEET; BLACK-HOLES; SPECTROMETER; PROTON; FLUX; PROGRESS; MODEL AB The BESS-Polar spectrometer had its first successful balloon flight over Antarctica in December 2004. During the 8.5-day long-duration flight, almost 0.9 billion events were recorded and 1,520 antiprotons were detected in the energy range 0.1-4.2 GeV. In this Letter, we report the antiproton spectrum obtained, discuss the origin of cosmic-ray antiprotons, and use antiproton data to probe the effect of charge-sign-dependent drift in the solar modulation. (C) 2008 Elsevier B.V. All rights reserved. C1 [Abe, K.; Itazaki, A.; Orito, R.; Shikaze, Y.; Takasugi, Y.; Takeuchi, K.] Kobe Univ, Kobe, Hyogo 6578501, Japan. [Fuke, H.; Yamagami, T.; Yoshida, T.] Japan Aerosp Explorat Agcy, Inst Space & Astronaut Sci, Sagamihara, Kanagawa 2298510, Japan. [Haino, S.; Kumazawa, T.; Makida, Y.; Matsuda, S.; Matsumoto, K.; Nozaki, M.; Suzuki, J.; Tanaka, K.; Yamamoto, A.; Yoshimura, K.] High Energy Accelerator Res Org, Tsukuba, Ibaraki 3050801, Japan. [Hams, T.; Mitchell, J. W.; Moiseev, A. A.; Sasaki, M.; Streitmatter, R. E.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Kim, K. C.; Lee, M. H.; Myers, Z.; Seo, E. S.] Univ Maryland, IPST, College Pk, MD 20742 USA. [Nishimura, J.] Univ Tokyo, Bunkyo Ku, Tokyo 1130033, Japan. [Ormes, J. F.] Univ Denver, Denver, CO 80208 USA. [Hams, T.; Sasaki, M.] CRESST USRA, Columbia, MD 21044 USA. RP Haino, S (reprint author), Ist Nazl Fis Nucl, I-06123 Perugia, Italy. EM haino@post.kek.jp OI Seo, Eun-Suk/0000-0001-8682-805X FU ISAS/JAXA; KEK; National Science Foundation (NSF), USA; Raytheon Polar Service Company; MEXT in Japan [KAKENHI-13001004, KAKENHI-15340077, KAKENHI-181040006]; NASA in the USA FX The authors thank NASA Headquarters for continuous encouragement in this US-Japan cooperative project. Sincere thanks are expressed to the NASA Balloon Programs Office at GSFC/WFF and to the NASA Columbia Scientific Balloon Facility for their experienced support. They also thank ISAS/JAXA and KEK for their continuous support and encouragement. Special thanks go to the National Science Foundation (NSF), USA, and Raytheon Polar Service Company for their professional support in the USA and in Antarctica. The authors would thank the BESS-Polar II collaborators M. Hasegawa, A. Horikoshi, K. Sakai, and N. Thakur for their contribution to the instrument performance evaluation and further cooperation. The BESS-Polar experiment is being carried out as a Japan-US Collaboration. It is supported by MEXT grants (KAKENHI-13001004, 15340077, and 181040006) in Japan, and by NASA grants in the USA. NR 45 TC 46 Z9 46 U1 0 U2 4 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0370-2693 J9 PHYS LETT B JI Phys. Lett. B PD DEC 11 PY 2008 VL 670 IS 2 BP 103 EP 108 DI 10.1016/j.physletb.2008.10.053 PG 6 WC Astronomy & Astrophysics; Physics, Nuclear; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA 385NJ UT WOS:000261820600002 ER PT J AU Tedder, SA Weikl, MC Seeger, T LeipertZ, A AF Tedder, Sarah A. Weikl, Markus C. Seeger, Thomas LeipertZ, Alfred TI Determination of probe volume dimensions in coherent measurement techniques SO APPLIED OPTICS LA English DT Article ID STOKES-RAMAN SCATTERING; SPECTROSCOPY; BOXCARS; FLAME AB When investigating combustion phenomena with pump-probe techniques, the spatial resolution is given by the overlapping region of the laser beams and thus defines the probe volume size. The size of this probe volume becomes important when the length scales of interest are on the same order or smaller. We present a new approach to measure the probe volume in three dimensions, which can be used to determine the probe volume length, diameter, and shape. The optical arrangement and data evaluation are demonstrated for a dual-pump dual-broadband coherent anti-Stokes Raman scattering setup that is used for combustion diagnostics. This new approach offers a simple, quick alternative with more capabilities than formerly used probe volume measurement methods. (c) 2008 Optical Society of America. C1 [Tedder, Sarah A.] NASA, Langley Res Ctr, Adv Sensing & Opt Measurement Branch, Hampton, VA 23681 USA. [Weikl, Markus C.; Seeger, Thomas; LeipertZ, Alfred] Lehrstuhl Tech Thermodynam, D-91058 Erlangen, Germany. [Weikl, Markus C.; Seeger, Thomas; LeipertZ, Alfred] Erlangen Grad Sch Adv Opt Technol SAOT, D-91052 Erlangen, Germany. RP Tedder, SA (reprint author), NASA, Langley Res Ctr, Adv Sensing & Opt Measurement Branch, 12 Langley Blvd, Hampton, VA 23681 USA. EM sarah.a.tedder@nasa.gov RI Seeger, Thomas/C-3951-2017; OI Seeger, Thomas/0000-0002-9145-5910; Weikl, Markus/0000-0002-8570-3842 FU School in Advanced Optical Technologies (SAOT); German National Science Foundation (DFG) FX The authors gratefully acknowledge funding of the Erlangen Graduate School in Advanced Optical Technologies (SAOT) by the German National Science Foundation (DFG) in the framework of the excellence initiative. The authors would also like to thank Greg Herring and Dimitrii Kozlov for advice and direction regarding CARS probe volume theory. NR 13 TC 12 Z9 12 U1 0 U2 1 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 DEC 10 PY 2008 VL 47 IS 35 BP 6601 EP 6605 DI 10.1364/AO.47.006601 PG 5 WC Optics SC Optics GA 391NR UT WOS:000262240500017 PM 19079469 ER PT J AU Vanderveld, RA AF Vanderveld, R. Ali TI QUANTIFYING PARAMETER ERRORS DUE TO THE PECULIAR VELOCITIES OF TYPE Ia SUPERNOVAE SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmological parameters; cosmology: observations; cosmology: theory; supernovae: general ID HIGH-REDSHIFT SUPERNOVAE; HUBBLE-SPACE-TELESCOPE; OMEGA(LAMBDA); CONSTRAINTS; EVOLUTION; OMEGA(M); SET AB The fitting of the observed redshifts and magnitudes of Type Ia supernovae to what we would see in homogeneous cosmological models has led to constraints on cosmological parameters. However, in performing such fits it is assumed that the sampled supernovae are moving with the Hubble flow, or namely that their peculiar velocities are zero. In reality, peculiar velocities will modify supernova data in a way that can impact best-fit cosmological parameters. We theoretically quantify this effect in the nonlinear regime with a Monte Carlo analysis, using data from semi-analytical galaxy catalogs built from the Millennium N-body simulation. We find scaling relations for the errors in best-fit parameters resulting solely from peculiar velocities, as a function of the total number of sources in a supernova survey N and its maximum redshift zmax. For low-redshift surveys, we find that these errors can be of the same order of magnitude as the errors due to an intrinsic magnitude scatter of 0.1 mag. For a survey with N = 2000 and z(max) = 1.7, we estimate that the expected peculiar velocity-induced errors in the best-fit cosmological constant density and equation of state can be sigma(Lambda) approximate to 0.009 and sigma(w) approximate to 0.01, respectively, which are subdominant to the errors due to the intrinsic scatter. We further find that throwing away supernova data below a redshift z approximate to 0.01-0.02 can reduce the combined error due to peculiar velocities and the intrinsic scatter, but by only about 10%. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Vanderveld, RA (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM rav@caltech.edu NR 15 TC 3 Z9 3 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD DEC 10 PY 2008 VL 689 IS 1 BP 49 EP 52 DI 10.1086/592396 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 401GV UT WOS:000262929000003 ER PT J AU Graff, PB Georganopoulos, M Perlman, ES Kazanas, D AF Graff, Philip B. Georganopoulos, Markos Perlman, Eric S. Kazanas, Demosthenes TI A MULTIZONE MODEL FOR SIMULATING THE HIGH-ENERGY VARIABILITY OF TeV BLAZARS SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: active; quasars: general; radiation mechanisms: nonthermal; X-rays: galaxies ID SELF-COMPTON MODEL; RAPID NONTHERMAL FLARES; BL LACERTAE OBJECTS; SIMULTANEOUS X-RAY; MULTIWAVELENGTH OBSERVATIONS; SPECTRAL EVOLUTION; MARKARIAN 421; PKS 2155-304; CORRELATED VARIABILITY; SYNCHROTRON EMISSION AB We present a time-dependent multizone code for simulating the variability of synchrotron self-Compton (SSC) sources. The code adopts a multizone pipe geometry for the emission region, appropriate for simulating emission from a standing or propagating shock in a collimated jet. Variations in the injection of relativistic electrons in the inlet propagate along the length of the pipe, cooling radiatively. Our code for the first time takes into account the nonlocal, time-retarded nature of SSC losses that are thought to be dominant in TeV blazars. The observed synchrotron and SSC emission is followed self-consistently, taking into account light-travel time delays. At any given time, the emitting portion of the pipe depends on the frequency and the nature of the variation followed. Our simulation employs only one additional physical parameter relative to one-zone models, that of the pipe length, and is computationally very efficient, using simplified expressions for the SSC processes. The code will be useful for observers modeling Fermi, TeV, and X-ray observations of SSC blazars. C1 [Graff, Philip B.; Georganopoulos, Markos] Univ Maryland, Joint Ctr Astrophys, Dept Phys, Baltimore, MD 21250 USA. [Georganopoulos, Markos; Kazanas, Demosthenes] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Perlman, Eric S.] Florida Inst Technol, Dept Phys & Space Sci, Melbourne, FL 32901 USA. RP Graff, PB (reprint author), Univ Maryland, Joint Ctr Astrophys, Dept Phys, 1000 Hilltop Circle, Baltimore, MD 21250 USA. OI Perlman, Eric/0000-0002-3099-1664 NR 44 TC 32 Z9 33 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD DEC 10 PY 2008 VL 689 IS 1 BP 68 EP 78 DI 10.1086/592427 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 401GV UT WOS:000262929000006 ER PT J AU Melendez, M Kraemer, SB Schmitt, HR Crenshaw, DM Deo, RP Mushotzky, RF Bruhweiler, FC AF Melendez, M. Kraemer, S. B. Schmitt, H. R. Crenshaw, D. M. Deo, R. P. Mushotzky, R. F. Bruhweiler, F. C. TI CONSTRAINING THE ACTIVE GALACTIC NUCLEUS CONTRIBUTION IN A MULTIWAVELENGTH STUDY OF SEYFERT GALAXIES SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: Seyfert; Galaxy: stellar content; infrared: galaxies ID SPITZER-SPACE-TELESCOPE; LUMINOUS INFRARED GALAXIES; NARROW-LINE REGION; X-RAY-EMISSION; STAR-FORMATION; MU-M; ENERGY-DISTRIBUTIONS; NEARBY GALAXIES; SAMPLE; SPECTRA AB We have studied the relationship between the high- and low-ionization [O IV] lambda 25.89 mu m, [Ne III] lambda 115.56 mu m, and [ Ne ii] lambda 12.81 mu m emission lines with the aim of constraining the active galactic nuclei (AGNs) and star formation contributions for a sample of 103 Seyfert galaxies. We use the [O iv] and [Ne ii] emission as tracers for the AGN power and star formation to investigate the ionization state of the emission- line gas. We find that Seyfert 2 galaxies have, on average, lower [O IV]/[ Ne II] ratios than Seyfert 1 galaxies. This result suggests two possible scenarios: (1) Seyfert 2 galaxies have intrinsically weakerAGNs, or (2) Seyfert 2 galaxies have relatively higher star formation rates than Seyfert 1 galaxies. We estimate the fraction of [Ne II] directly associated with the AGNs and find that Seyfert 2 galaxies have a larger contribution from star formation, by a factor of similar to 1.5 on average, than what is found in Seyfert 1 galaxies. Using the stellar component of [Ne II] as a tracer of the current star formation, we found similar star formation rates in Seyfert 1 and Seyfert 2 galaxies. We examined the mid- and far- infrared continua and found that [Ne II] iswell correlatedwith the continuum luminosity at 60 mu m and that both [Ne III] and [O IV] are better correlated with the 25 mu m luminosities than with the continuum at longer wavelengths, suggesting that the mid- infrared continuum luminosity is dominated by the AGN, while the far- infrared luminosity is dominated by star formation. Overall, these results test the unified model of AGNs and suggest that the differences between Seyfert galaxies cannot be solely due to viewing angle dependence. C1 [Melendez, M.; Kraemer, S. B.; Bruhweiler, F. C.] Catholic Univ Amer, Dept Phys, Inst Astrophys & Computat Sci, Washington, DC 20064 USA. [Schmitt, H. R.] USN, Res Lab, Remote Sensing Div, Washington, DC 20375 USA. [Schmitt, H. R.] Interferometrics Inc, Herndon, VA 20171 USA. [Crenshaw, D. M.] Georgia State Univ, Dept Phys & Astron, Atlanta, GA 30302 USA. [Deo, R. P.] Drexel Univ, Dept Phys, Philadelphia, PA 19104 USA. [Mushotzky, R. F.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Melendez, M (reprint author), Catholic Univ Amer, Dept Phys, Inst Astrophys & Computat Sci, Washington, DC 20064 USA. EM 07melendez@cua.edu NR 63 TC 47 Z9 47 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD DEC 10 PY 2008 VL 689 IS 1 BP 95 EP 107 DI 10.1086/592724 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 401GV UT WOS:000262929000008 ER PT J AU Marrero, AYR Torres, DF del Pozo, ED Reimer, O Cillis, AN AF Rodriguez Marrero, Ana Y. Torres, Diego F. de Cea del Pozo, Elsa Reimer, Olaf Cillis, Analia N. TI DIFFUSION OF COSMIC RAYS AND THE GAMMA-RAY LARGE AREA TELESCOPE: PHENOMENOLOGY AT THE 1-100 GeV REGIME SO ASTROPHYSICAL JOURNAL LA English DT Article DE gamma rays: observations; gamma rays: theory ID EMISSION; RADIATION; EGRET AB This paper analyzes astrophysical scenarios that may be detected at the upper end of the energy range of the Gamma-Ray Large Area Space Telescope (GLAST), as a result of cosmic-ray (CR) diffusion in the interstellar medium (ISM). Hadronic processes are considered the source of gamma-ray photons from localized molecular enhancements nearby accelerators. Two particular cases are presented: (1) the possibility of detecting spectral energy distributions (SEDs) with maxima above 1 GeV, which may be constrained by detection or nondetection at very high energies (VHEs) with observations by ground-based Cerenkov telescopes, and (2) the possibility of detecting V-shaped, inverted spectra, due to confusion of a nearby (to the line of sight) arrangement of accelerator/target scenarios with different characteristic properties. We show that finding these signatures (in particular, a peak at the 1-100 GeVenergy region) indicates the underlying mechanism producing the gamma-rays that is realized by nature, which accelerator (age and relative position to the target cloud) and under which diffusion properties CRs propagate. C1 [Rodriguez Marrero, Ana Y.; Torres, Diego F.; de Cea del Pozo, Elsa] Campus UAB, Fac Sci, Inst Ciencies Espai, IEEC CSIC, Barcelona 08193, Spain. [Reimer, Olaf] Stanford Univ, WW Hansen Expt Phys Lab HEPL, Stanford, CA 94305 USA. [Reimer, Olaf] Stanford Univ, KIPAC, Stanford, CA 94305 USA. [Cillis, Analia N.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Marrero, AYR (reprint author), Campus UAB, Fac Sci, Inst Ciencies Espai, IEEC CSIC, Torre C5,Parell,2a Planta, Barcelona 08193, Spain. EM arodrig@ieec.uab.es; decea@ieec.uab.es; dtorres@ieec.uab.es; olr@stanford.edu; analia.n.cillis@nasa.gov RI Reimer, Olaf/A-3117-2013; Torres, Diego/O-9422-2016 OI Reimer, Olaf/0000-0001-6953-1385; Torres, Diego/0000-0002-1522-9065 NR 16 TC 13 Z9 13 U1 0 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD DEC 10 PY 2008 VL 689 IS 1 BP 213 EP 218 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 401GV UT WOS:000262929000018 ER PT J AU Katsuda, S Tsunemi, H Uchida, H Kimura, M AF Katsuda, S. Tsunemi, H. Uchida, H. Kimura, M. TI FORWARD SHOCK PROPER MOTIONS OF KEPLER'S SUPERNOVA REMNANT SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM: individual (Kepler's Supernova); shock waves; supernova remnants; X-rays: ISM ID X-RAY; EXPANSION; EMISSION; EVOLUTION AB The X-ray structure of Kepler's supernova remnant shows a rounded shape delineated by forward shocks. We measure proper motions of the forward shocks on overall rims of the remnant, by using archival Chandra data taken in two epochs with time difference of 6.09 yr. The proper motions of the forward shocks on the northern rim are measured to be 0.076 '' (+/- 0.032 '' +/- 0.016 '') to 0.11 '' (+/- 0.014 '' +/- 0.016 '') yr(-1), while those on the rest of the rims are measured to be 0.15 '' (+/- 0.017 '' +/- 0.016 '') to 0.30 '' (+/- 0.048 '' +/- 0.016 '') yr(-1); here the first-termerrors are statistical uncertainties and the second-term errors are systematic uncertainties. Combining the best-estimated shock velocity of 1660 +/- 120 km s(-1) measured for Balmer-dominated filaments in the northern and central portions of the remnant (Sankrit et al. 2005) with the proper motions derived for the forward shocks on the northern rim, we estimate a distance of 3.3(-0.4)(+1.6) kpc to the remnant. We measure the expansion indices, m (defined as R alpha t(m)), to be 0.47-0.82 for most of the rims. These values are consistent with those expected in Type Ia SN explosion models, in which the ejecta and the circumstellar medium have power-law density profiles whose indices are 5-7 and 0-2, respectively. In addition, we should note the slower expansion on the northern rim than that on the southern rim. This is likely caused by the inhomogeneous circumstellar medium; the density of the circumstellar medium is higher in the north than that in the south of the remnant. The newly estimated geometric center, around which we believe the explosion point exists, is located at similar to 5 '' offset to the north of the radio center. C1 [Katsuda, S.; Tsunemi, H.; Uchida, H.; Kimura, M.] Osaka Univ, Grad Sch Sci, Dept Earth & Space Sci, Osaka 5600043, Japan. [Katsuda, S.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Katsuda, S (reprint author), Osaka Univ, Grad Sch Sci, Dept Earth & Space Sci, 1-1 Machikaneyama, Osaka 5600043, Japan. EM satoru.katsuda@nasa.gov; tsunemi@ess.sci.osaka-u.ac.jp; uchida@ess.sci.osaka-u.ac.jp; mkimura@ess.sci.osaka-u.ac.jp NR 25 TC 12 Z9 12 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD DEC 10 PY 2008 VL 689 IS 1 BP 225 EP 230 DI 10.1086/592376 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 401GV UT WOS:000262929000020 ER PT J AU Krco, M Goldsmith, PF Brown, RL Li, D AF Krco, Marko Goldsmith, Paul F. Brown, Robert L. Li, D. TI AN IMPROVED TECHNIQUE FOR MEASUREMENT OF COLD H I IN MOLECULAR CLOUD CORES SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM: clouds; ISM: evolution; line: profiles; molecular processes ID NARROW SELF-ABSORPTION; GALACTIC PLANE SURVEY; DARK CLOUDS; NEUTRAL HYDROGEN; ATOMIC-HYDROGEN; RADIO-CONTINUUM; DUST; TAURUS; GAS; COMPLEX AB The presence of atomic gas mixed with molecular species in a "molecular" cloud may significantly affect its chemistry, the excitation of some species, and can serve as probe of the cloud's evolution. Cold neutral atomic hydrogen (H I) in molecular clouds is revealed by its self absorption of background galactic H I 21 cm emission. The properties of this gas can be investigated quantitatively through observation of H I narrow self-absorption (HINSA). In this paper we present a new technique for measuring atomic gas physical parameters from HINSA observations that utilizes molecular tracers to guide the HINSA extraction. This technique offers a significant improvement in the precision with which H I column densities can be determined over previous methods, and it opens several new avenues of study of relevance to the field of star formation. C1 [Krco, Marko; Goldsmith, Paul F.] Cornell Univ, Dept Astron, Ithaca, NY 14853 USA. [Goldsmith, Paul F.; Li, D.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Brown, Robert L.] Cornell Univ, Natl Astron & Ionosphere Ctr, Ithaca, NY 14853 USA. RP Krco, M (reprint author), Cornell Univ, Dept Astron, Ithaca, NY 14853 USA. EM marko@astro.cornell.edu RI Goldsmith, Paul/H-3159-2016 NR 26 TC 11 Z9 11 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD DEC 10 PY 2008 VL 689 IS 1 BP 276 EP 289 DI 10.1086/592553 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 401GV UT WOS:000262929000025 ER PT J AU Liu, Y Luhmann, JG Muller-Mellin, R Schroeder, PC Wang, L Lin, RP Bale, SD Li, Y Acuna, MH Sauvaud, JA AF Liu, Y. Luhmann, J. G. Mueller-Mellin, R. Schroeder, P. C. Wang, L. Lin, R. P. Bale, S. D. Li, Y. Acuna, M. H. Sauvaud, J. -A. TI A COMPREHENSIVE VIEW OF THE 2006 DECEMBER 13 CME: FROM THE SUN TO INTERPLANETARY SPACE SO ASTROPHYSICAL JOURNAL LA English DT Article DE shock waves; solar-terrestrial relations; solar wind; Sun: coronal mass ejections (CMEs); Sun: particle emission; Sun: radio radiation ID CORONAL MASS EJECTIONS; MAGNETIC-FIELD; SOLAR-WIND; RADIO; EMISSION; ULYSSES; PROPAGATION; ELECTRONS; ORIGIN; EVENT AB The biggest halo coronal mass ejection (CME) since the Halloween storm in 2003, which occurred on 2006 December 13, is studied in terms of its solar source and heliospheric consequences. The CME was accompanied by an X3.4 flare, EUV dimmings, and coronal waves. It generated significant space weather effects such as an interplanetary shock, radio bursts, major solar energetic particle (SEP) events, and a magnetic cloud (MC) that were detected by a fleet of spacecraft including STEREO, ACE, WIND, and Ulysses. Reconstruction of the MC with the Grad-Shafranov (GS) method yields an axis orientation oblique to the flare ribbons. Observations of the SEP intensities and anisotropies show that the particles can be trapped, deflected, and reaccelerated by the large-scale transient structures. The CME-driven shock was observed at both the Earth and Ulysses when they were separated by 74 degrees in latitude and 117 degrees in longitude, which is the largest shock extent ever detected. The ejecta seem to have been missed at Ulysses. The shock arrival time at Ulysses is well predicted by an MHD model that can propagate the 1 AU data outward. The CME/shock is tracked remarkably well from the Sun all the way to Ulysses by coronagraph images, type II frequency drift, in situ measurements, and the MHD model. These results reveal a technique that combines MHD propagation of the solar wind and type II emissions to predict the shock arrival time at the Earth, which is a significant advance for space weather forecasting, especially when in situ data become available from the Solar Orbiter and Solar Sentinels. C1 [Liu, Y.; Luhmann, J. G.; Schroeder, P. C.; Wang, L.; Lin, R. P.; Bale, S. D.; Li, Y.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Liu, Y.] Chinese Acad Sci, State Key Lab Space Weather, Beijing 100080, Peoples R China. [Mueller-Mellin, R.] Univ Kiel, Inst Expt & Angewandte Phys, D-24098 Kiel, Germany. [Acuna, M. H.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Sauvaud, J. -A.] CNRS, Ctr Etud Spatiale Rayonnements, F-31028 Toulouse 4, France. RP Liu, Y (reprint author), Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. EM liuxying@ssl.berkeley.edu RI Bale, Stuart/E-7533-2011; Wang, Linghua/C-4938-2014; OI Bale, Stuart/0000-0002-1989-3596; Wang, Linghua/0000-0001-7309-4325; Liu, Ying/0000-0002-3483-5909 FU STEREO [NAS5-03131]; NNSFC [40621003] FX The research was supported by the STEREO project under grant NAS5-03131. We acknowledge the use of SOHO, GOES, ACE, WIND, and Ulysses data and CME parameters from the LASCO CME catalog maintained by NASA and the Catholic University of America in cooperation with the Naval Research Laboratory ( RL). We thank C. T. Russell for helping to maintain the STEREOMAG data and are grateful to the referee for his or her helpful suggestions. This work was also supported in part by grant NNSFC 40621003. NR 47 TC 55 Z9 58 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 DEC 10 PY 2008 VL 689 IS 1 BP 563 EP 571 DI 10.1086/592031 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 401GV UT WOS:000262929000049 ER PT J AU Remijan, AJ Milam, SN Womack, M Apponi, AJ Ziurys, LM Wyckoff, S A'Hearn, MF de Pater, I Forster, JR Friedel, DN Palmer, P Snyder, LE Veal, JM Woodney, LM Wright, MCH AF Remijan, Anthony J. Milam, Stefanie N. Womack, Maria Apponi, A. J. Ziurys, L. M. Wyckoff, Susan A'Hearn, M. F. de Pater, Imke Forster, J. R. Friedel, D. N. Palmer, Patrick Snyder, L. E. Veal, J. M. Woodney, L. M. Wright, M. C. H. TI THE DISTRIBUTION, EXCITATION, AND FORMATION OF COMETARY MOLECULES: METHANOL, METHYL CYANIDE, AND ETHYLENE GLYCOL SO ASTROPHYSICAL JOURNAL LA English DT Article DE astrobiology; comets: individual (Hale Bopp [C/1995 01], LINEAR [C/2002 T7]); molecular processes; radio lines: solar system; techniques: interferometric ID O1 HALE-BOPP; C/1995 O1; C/2001 Q4; SPECTROSCOPY; FORMALDEHYDE; REGIONS; CH3CN; CORE; NEAT; HOT AB We present an interferometric and single-dish study of small organic species toward Comets C/1995 O1 (Hale-Bopp) and C/2002 T7 (LINEAR) using the BIMA interferometer at 3 mm and the ARO 12 m telescope at 2 mm. For Comet Hale-Bopp, both the single-dish and interferometer observations of CH(3)OH indicate an excitation temperature of 105 +/- 5 K and an average production rate ratio Q(CH(3)OH)/Q(H(2)O) similar to 1.3% at similar to 1 AU. In addition, the aperture synthesis observations of CH(3)OH suggest a distribution well described by a spherical outflow and no evidence of significant extended emission. Single-dish observations of CH(3)CN in Comet Hale-Bopp indicate an excitation temperature of 200 +/- 10 K and a production rate ratio of Q(CH(3)CN)/Q(H(2)O) similar to 0.017% at similar to 1 AU. The nondetection of a previously claimed transition of cometary (CH(2)OH)(2) toward Comet Hale-Bopp with the 12 m telescope indicates a compact distribution of emission, D < 9 '' (< 8500 km). For the single-dish observations of Comet T7 LINEAR, we find an excitation temperature of CH(3)OH of 35 +/- 5 K and a CH(3)OH production rate ratio of Q(CH(3)OH)/Q(H(2)O) similar to 1.5% at similar to 0.3 AU. Our data support current chemical models that CH(3)OH, CH(3)CN, and (CH(2)OH)(2) are parent nuclear species distributed into the coma via direct sublimation off cometary ices from the nucleus with no evidence of significant production in the outer coma. C1 [Remijan, Anthony J.] Natl Radio Astron Observ, Charlottesville, VA 22901 USA. [Milam, Stefanie N.; Apponi, A. J.; Ziurys, L. M.] Univ Arizona, Dept Chem, NASA, Astrobiol Inst, Tucson, AZ 85721 USA. [Womack, Maria] St Cloud State Univ, Dept Phys & Astron, St Cloud, MN 56301 USA. [Wyckoff, Susan] Arizona State Univ, Dept Phys & Astron, Tempe, AZ 85287 USA. [A'Hearn, M. F.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [de Pater, Imke; Forster, J. R.; Wright, M. C. H.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Friedel, D. N.; Snyder, L. E.; Veal, J. M.] Univ Illinois, Dept Astron, Urbana, IL 61801 USA. [Palmer, Patrick] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA. [Woodney, L. M.] Calif State Univ San Bernardino, Dept Phys, San Bernardino, CA 92407 USA. RP Remijan, AJ (reprint author), Natl Radio Astron Observ, 520 Edgemont Rd, Charlottesville, VA 22901 USA. EM aremijan@nrao.edu; stefanie.n.milam@nasa.gov; mwomack@stcloudstate.edu; aapponi@as.arizona.edu; lziurys@as.arizona.edu; wyckoff@asu.edu; ma@astro.umd.edu; imke@floris.berkeley.edu; rforster@astro.berkeley.edu; friedel@astro.uiuc.edu; ppalmer@oskar.uchicago.edu; snyder@astro.uiuc.edu; jveal@swccd.edu; woodney@csusb.edu; wright@astro.berkeley.edu RI Milam, Stefanie/D-1092-2012; OI Milam, Stefanie/0000-0001-7694-4129; Womack, Maria/0000-0003-4659-8653 NR 35 TC 9 Z9 9 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD DEC 10 PY 2008 VL 689 IS 1 BP 613 EP 621 DI 10.1086/592242 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 401GV UT WOS:000262929000053 ER PT J AU Bentz, MC Walsh, JL Barth, AJ Baliber, N Bennert, N Canalizo, G Filippenko, AV Ganeshalingam, M Gates, EL Greene, JE Hidas, MG Hiner, KD Lee, N Li, WD Malkan, MA Minezaki, T Serduke, FJD Shiode, JH Silverman, JM Steele, TN Stern, D Street, RA Thornton, CE Treu, T Wang, XF Woo, JH Yoshii, Y AF Bentz, Misty C. Walsh, Jonelle L. Barth, Aaron J. Baliber, Nairn Bennert, Nicola Canalizo, Gabriela Filippenko, Alexei V. Ganeshalingam, Mohan Gates, Elinor L. Greene, Jenny E. Hidas, Marton G. Hiner, Kyle D. Lee, Nicholas Li, Weidong Malkan, Matthew A. Minezaki, Takeo Serduke, Frank J. D. Shiode, Joshua H. Silverman, Jeffrey M. Steele, Thea N. Stern, Daniel Street, Rachel A. Thornton, Carol E. Treu, Tommaso Wang, Xiaofeng Woo, Jong-Hak Yoshii, Yuzuru TI FIRST RESULTS FROM THE LICK AGN MONITORING PROJECT: THE MASS OF THE BLACK HOLE IN ARP 151 SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE galaxies: active; galaxies: individual (Arp 151); galaxies: nuclei; galaxies: Seyfert ID ACTIVE GALACTIC NUCLEI; BROAD-LINE REGION; SEYFERT-GALAXIES; EMISSION; REVERBERATION; VARIABILITY; CONTINUUM; NGC-5548; QUASARS; SIZES AB We have recently completed a 64 night spectroscopic monitoring campaign at the Lick Observatory 3 m Shane telescope with the aim of measuring the masses of the black holes in 13 nearby (z < 0.05) Seyfert 1 galaxies with with expected masses in the range similar to 10(6)-10(7) M(circle dot). We present here the first results from this project-the mass, of the central black hole in Arp 151. Strong variability throughout the campaign led to an exceptionally clean H beta lag measurement in this object of 4.25(-0.66)(+0.68) days in the observed frame. Coupled with the width of the H beta emission line in the variable spectrum, we determine a black hole mass of (7.1 +/- 1.2) x 10(6) M(circle dot), assuming the Onken et al. normalization for reverberation-based virial masses. We also find velocity-resolved lag information within the H beta emission line which clearly shows infalling gas in the H beta-emitting region. Further detailed analysis may lead to a full model of the geometry and kinematics of broad line region gas around the central black hole in Arp 151. C1 [Bentz, Misty C.; Walsh, Jonelle L.; Barth, Aaron J.; Thornton, Carol E.] Univ Calif Irvine, Dept Phys & Astron, Irvine, CA 92697 USA. [Baliber, Nairn; Bennert, Nicola; Hidas, Marton G.; Street, Rachel A.; Treu, Tommaso; Woo, Jong-Hak] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA. [Baliber, Nairn; Hidas, Marton G.; Street, Rachel A.] Las Cumbres Observ Global Telescope, Goleta, CA 93117 USA. [Bennert, Nicola; Canalizo, Gabriela; Hiner, Kyle D.] Univ Calif Riverside, Inst Geophys & Planetary Phys, Riverside, CA 92521 USA. [Canalizo, Gabriela; Hiner, Kyle D.] Univ Calif Riverside, Dept Phys & Astron, Riverside, CA 92521 USA. [Filippenko, Alexei V.; Ganeshalingam, Mohan; Lee, Nicholas; Li, Weidong; Serduke, Frank J. D.; Shiode, Joshua H.; Silverman, Jeffrey M.; Steele, Thea N.; Wang, Xiaofeng] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Gates, Elinor L.] Lick Observ, Mt Hamilton, CA 95140 USA. [Greene, Jenny E.] Princeton Univ Observ, Princeton, NJ 08544 USA. [Malkan, Matthew A.; Woo, Jong-Hak] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90024 USA. [Minezaki, Takeo; Yoshii, Yuzuru] Univ Tokyo, Sch Sci, Inst Astron, Tokyo 1810015, Japan. [Stern, Daniel] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Wang, Xiaofeng] Tsinghua Univ, Dept Phys, Beijing 100084, Peoples R China. [Wang, Xiaofeng] Tsinghua Univ, Tsinghua Ctr Astrophys THCA, Beijing 100084, Peoples R China. [Yoshii, Yuzuru] Univ Tokyo, Sch Sci, Res Ctr Early Univ, Tokyo 1130033, Japan. RP Bentz, MC (reprint author), Univ Calif Irvine, Dept Phys & Astron, 4129 Frederick Reines Hall, Irvine, CA 92697 USA. EM mbentz@uci.edu RI Woo, Jong-Hak/A-2790-2014; Wang, Xiaofeng/J-5390-2015 FU NSF [AST 0548198, AST 0607485, AST 0642621, AST 0507450]; TABASGO Foundation FX We thank the Lick Observatory staff for their tireless support during this project. We also thank Brad Peterson for helpful conversations and the use of his analysis software. This work was supported by NSF grants AST 0548198 (UC Irvine), AST 0607485 (UC Berkeley), AST 0642621 (UC Santa Barbara), and AST 0507450 (UC Riverside), as well as the TABASGO Foundation (UC Berkeley). NR 23 TC 40 Z9 40 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD DEC 10 PY 2008 VL 689 IS 1 BP L21 EP L24 DI 10.1086/595719 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 398LO UT WOS:000262733800006 ER PT J AU Burgasser, AJ Tinney, CG Cushing, MC Saumon, D Marley, MS Bennett, CS Kirkpatrick, JD AF Burgasser, Adam J. Tinney, C. G. Cushing, Michael C. Saumon, Didier Marley, Mark S. Bennett, Clara S. Kirkpatrick, J. Davy TI 2MASS J09393548-2448279: THE COLDEST AND LEAST LUMINOUS BROWN DWARF BINARY KNOWN? SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE binaries: close; stars: fundamental parameters; stars: individual (2MASS J04151954-0935066 2MASS J09393548-2448279); stars: low-mass, brown dwarfs ID SPITZER-SPACE-TELESCOPE; INFRARED ARRAY CAMERA; T-DWARFS; SPECTRAL CLASSIFICATION; ADAPTIVE OPTICS; FILTER SET; SPECTROGRAPH; TRANSITION; SEARCH; ATMOSPHERES AB Determinations of the luminosity and atmospheric properties of the T8 brown dwarf 2MASS J09393548 - 2448279 are presented, based on Spitzer IRAC and IRS observations and ground-based astrometry. We find log(10) (L(bol)/L(circle dot)) = -5.69 +/- 0.03 for this source, comparable to the current low-luminosity record holder 2MASS J04151954 - 0935066. However, modeling of near- and mid-infrared spectral data indicates an effective temperature of 600 +/- 35 K, roughly 100 K cooler than 2M0415. These parameters require a highly inflated radius for 2M0939 (R approximate to 0.13 R(circle dot)) which cannot be reconciled with brown dwarf structure models. However, if this source is an unresolved, equal-mass binary, then the reduced luminosity of each component (L(bol) approximate to 10(-6) L(circle dot)) can be brought into agreement with the inferred atmospheric parameters for an age of 0.4-12 Gyr and component masses of 0.01-0.05 M(circle dot). This hypothesis can be tested through future high-resolution imaging and/or spectroscopic observations. C1 [Burgasser, Adam J.; Bennett, Clara S.] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. [Tinney, C. G.] Univ New S Wales, Sch Phys, Dept Astrophys, Sydney, NSW 2052, Australia. [Saumon, Didier] Los Alamos Natl Lab, Div Appl Phys, Los Alamos, NM 87545 USA. [Marley, Mark S.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Kirkpatrick, J. Davy] CALTECH, Infrared Proc Anal Ctr, Pasadena, CA 91125 USA. RP Burgasser, AJ (reprint author), MIT, Kavli Inst Astrophys & Space Res, Bldg 37,Room 664B,77 Massachusetts Ave, Cambridge, MA 02139 USA. EM ajb@mit.edu RI Marley, Mark/I-4704-2013 FU NASA [DP0774000]; NSF FX This publication makes use of data from the Two Micron All Sky Survey (2MASS), which is a joint project of the University of Massachusetts and the Infrared Processing and Analysis Center (IPAC), and funded by NASA and the NSF. The 2MASS data were obtained from the NASA/IPAC Infrared Science Archive, which is operated by the Jet Propulsion Laboratory, California Institute of Technology (JPL/Caltech), under contract with NASA. This work is also based in part on observations made with the Spitzer Space Telescope, which is operated by JPL/Caltech under a contract with NASA. Support for this work was provided by NASA through an award issued by JPL/Caltech. C. G. T. acknowledges support from ARC grant DP0774000. Support for D. S.'s work, part of the Spitzer Space Telescope Theoretical Research Program, was provided by NASA. We thank our anonymous referee for her/his prompt review of our original manuscript. NR 35 TC 31 Z9 31 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD DEC 10 PY 2008 VL 689 IS 1 BP L53 EP L56 DI 10.1086/595747 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 398LO UT WOS:000262733800014 ER PT J AU Meijerink, R Poelman, DR Spaans, M Tielens, AGGM Glassgold, AE AF Meijerink, R. Poelman, D. R. Spaans, M. Tielens, A. G. G. M. Glassgold, A. E. TI ROTATIONAL LINE EMISSION FROM WATER IN PROTOPLANETARY DISKS SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE accretion, accretion disks; infrared: stars; planetary systems: protoplanetary disks; radiative transfer; stars: pre-main-sequence; X-rays: stars ID ACCRETION DISKS; SNOW LINE; GAS TEMPERATURE; YOUNG OBJECTS; H2O; IRRADIATION; EXCITATION; LOCATION; REGION; MODELS AB Circumstellar disks provide the material reservoir for the growth of young stars and for planet formation. We combine a high-level radiative transfer program with a thermal-chemical model of a typical T Tauri star disk to investigate the diagnostic potential of the far-infrared lines of water for probing disk structure. We discuss the observability of pure rotational H(2)O lines with the Herschel Space Observatory, specifically the residual gas where water is mainly frozen out. We find that measuring both the line profile of the ground 1(10)-1(01) ortho-H(2)O transition and the ratio of this line to the 3(12)-3(03) and 2(21)-2(12) lines can provide information on the gas-phase water between 5 and 100 AU, but not on the snow line which is expected to occur at smaller radii. C1 [Meijerink, R.; Glassgold, A. E.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Poelman, D. R.] Univ St Andrews, Sch Phys & Astron, St Andrews KY16 9SS, Scotland. [Spaans, M.; Tielens, A. G. G. M.] Univ Groningen, Kapteyn Astron Inst, NL-9700 AV Groningen, Netherlands. [Tielens, A. G. G. M.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Meijerink, R (reprint author), Univ Calif Berkeley, Dept Astron, 601 Campbell Hall, Berkeley, CA 94720 USA. EM rowin@gps.caltech.edu FU NSF [AST 05-07423]; NASA [NNG06GF88G] FX This work has been supported by NSF grant AST 05-07423 and NASA grant NNG06GF88G to UC Berkeley. We thank F. van der Tak, P. d'Alessio, and the anonymous referee for their invaluable contributions. NR 26 TC 13 Z9 13 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD DEC 10 PY 2008 VL 689 IS 1 BP L57 EP L60 DI 10.1086/595726 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 398LO UT WOS:000262733800015 ER PT J AU Comstock, JM Lin, RF Starr, DO Yang, P AF Comstock, Jennifer M. Lin, Ruei-Fong Starr, David O'C. Yang, Ping TI Understanding ice supersaturation, particle growth, and number concentration in cirrus clouds SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Review ID WATER-VAPOR MEASUREMENTS; DELIQUESCENT MIXED CCN; ART. NO. 2230; IN-SITU DATA; RELATIVE-HUMIDITY; RADIATIVE PROPERTIES; CLIMATE MODELS; MICROPHYSICAL PROPERTIES; UPPER-TROPOSPHERE; RAMAN LIDAR AB Many factors control the ice supersaturation and microphysical properties in cirrus clouds. We explore the effects of dynamic forcing, ice nucleation mechanisms, and ice crystal growth rate on the evolution and distribution of water vapor and cloud properties in nighttime cirrus clouds using a one-dimensional cloud model with bin microphysics and remote sensing measurements obtained at the Department of Energy's Atmospheric Radiation Measurement (ARM) Climate Research Facility located near Lamont, OK. We forced the model using both large-scale vertical ascent and, for the first time, mean mesoscale velocity derived from radar Doppler velocity measurements. Both heterogeneous and homogeneous nucleation processes are explored, where a classical theory heterogeneous scheme is compared with empirical representations. We evaluated model simulations by examining both bulk cloud properties and distributions of measured radar reflectivity, lidar extinction, and water vapor profiles, as well as retrieved cloud microphysical properties. Our results suggest that mesoscale variability is the primary mechanism needed to reproduce observed quantities. Model sensitivity to the ice growth rate is also investigated. The most realistic simulations as compared with observations are forced using mesoscale waves, include fast ice crystal growth, and initiate ice by either homogeneous or heterogeneous nucleation. Simulated ice crystal number concentrations (tens to hundreds particles per liter) are typically two orders of magnitude smaller than previously published results based on aircraft measurements in cirrus clouds, although higher concentrations are possible in isolated pockets within the nucleation zone. C1 [Comstock, Jennifer M.] Pacific NW Natl Lab, Atmospher Sci & Global Change Div, Richland, WA 99352 USA. [Lin, Ruei-Fong] Univ Maryland, NASA, Goddard Space Flight Ctr, Goddard Earth Sci & Technol Ctr, Greenbelt, MD 20771 USA. [Starr, David O'C.] NASA, Goddard Space Flight Ctr, Atmospher & Space Phys Lab, Greenbelt, MD 20771 USA. [Yang, Ping] Texas A&M Univ, Dept Atmospher Sci, College Stn, TX 77843 USA. RP Comstock, JM (reprint author), Pacific NW Natl Lab, Atmospher Sci & Global Change Div, POB 999,MSIN K9-24, Richland, WA 99352 USA. EM jennifer.comstock@pnl.gov RI Yang, Ping/B-4590-2011 FU DOE Office of Science; Atmospheric Radiation Measurement (ARM) Program FX Research performed by Jennifer M. Comstock was supported by the DOE Office of Science, Atmospheric Radiation Measurement (ARM) Program. NR 101 TC 23 Z9 23 U1 3 U2 21 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 DEC 10 PY 2008 VL 113 IS D23 AR D23211 DI 10.1029/2008JD010332 PG 20 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 383JO UT WOS:000261670100009 ER PT J AU Stephens, GL Vane, DG Tanelli, S Im, E Durden, S Rokey, M Reinke, D Partain, P Mace, GG Austin, R L'Ecuyer, T Haynes, J Lebsock, M Suzuki, K Waliser, D Wu, D Kay, J Gettelman, A Wang, Z Marchand, R AF Stephens, Graeme L. Vane, Deborah G. Tanelli, Simone Im, Eastwood Durden, Stephen Rokey, Mark Reinke, Don Partain, Philip Mace, Gerald G. Austin, Richard L'Ecuyer, Tristan Haynes, John Lebsock, Matthew Suzuki, Kentaroh Waliser, Duane Wu, Dong Kay, Jen Gettelman, Andrew Wang, Zhien Marchand, Rojer TI CloudSat mission: Performance and early science after the first year of operation SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID COMMUNITY ATMOSPHERE MODEL; RADIATIVE PROPERTIES; MICROPHYSICS SCHEME; CLIMATE SYSTEM; VERSION-3 CAM3; RADAR; AIRBORNE; PRECIPITATION; CLOUDINESS; SPACE AB This paper reports on the early mission performance of the radar and other major aspects of the CloudSat mission. The Cloudsat cloud profiling radar (CPR) has been operating since 2 June 2006 and has proven to be remarkably stable since turn-on. A number of products have been developed using these space-borne radar data as principal inputs. Combined with other A-Train sensor data, these new observations offer unique, global views of the vertical structure of clouds and precipitation jointly. Approximately 11% of clouds detected over the global oceans produce precipitation that, in all likelihood, reaches the surface. Warm precipitating clouds are both wetter and composed of larger particles than nonprecipitating clouds. The frequency of precipitation increases significantly with increasing cloud depth, and the increased depth and water path of precipitating clouds leads to increased optical depths and substantially more sunlight reflected from precipitating clouds compared to than nonprecipitating warm clouds. The CloudSat observations also provide an authoritative estimate of global ice water paths. The observed ice water paths are larger than those predicted from most climate models. CloudSat observations also indicate that clouds radiatively heat the global mean atmospheric column (relative to clear skies) by about 10 Wm(-2). Although this heating appears to be contributed almost equally by solar and infrared absorption, the latter contribution is shown to vary significantly with latitude being influenced by the predominant cloud structures of the different region in questions. C1 [Stephens, Graeme L.; Austin, Richard; L'Ecuyer, Tristan; Haynes, John; Lebsock, Matthew; Suzuki, Kentaroh] Colorado State Univ, Dept Atmospher Sci, Ft Collins, CO 80523 USA. [Vane, Deborah G.; Tanelli, Simone; Im, Eastwood; Durden, Stephen; Rokey, Mark; Waliser, Duane; Wu, Dong] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Kay, Jen; Gettelman, Andrew] Natl Ctr Atmospher Res, Boulder, CO 80305 USA. [Mace, Gerald G.] Univ Utah, Dept Meteorol, Salt Lake City, UT 84112 USA. [Marchand, Rojer] Univ Washington, Joint Inst Study Atmosphere & Ocean, Seattle, WA 98195 USA. [Partain, Philip] MetSat, Sci Technol Corp, Ft Collins, CO 80323 USA. [Reinke, Don] Colorado State Univ, CIRA, Ft Collins, CO 80523 USA. [Wang, Zhien] Univ Wyoming, Dept Atmospher Sci, Laramie, WY 82071 USA. RP Stephens, GL (reprint author), Colorado State Univ, Dept Atmospher Sci, Ft Collins, CO 80523 USA. EM stephens@atmos.colostate.edu; dvane@jpl.nasa.gov; simone.tanelli@jpl.nasa.gov; eastwood.im@jpl.nasa.gov; stephen.durden@jpl.nasa.gov; mark.rokey@jpl.nasa.gov; reinke@cira.colostate.edu; partain@cira.colostate.edu; mace@met.utah.edu; Austin@atmos.colostate.edu; Tristan@atmos.colostate.edu; Haynes@atmos.colostate.edu; lebsock@atmos.colostate.edu; kenta@atmos.colostate.edu; duane.waliser@jpl.nasa.gov; Dong.L.Wu@jpl.nasa.gov; jenkay@cgd.ucar.edu; andrew@ucar.edu; zwang@uwyo.edu; rojmarch@u.washington.edu RI Suzuki, Kentaroh/C-3624-2011; Wang, Zhien/F-4857-2011; Kay, Jennifer/C-6042-2012; L'Ecuyer, Tristan/C-7040-2013; L'Ecuyer, Tristan/E-5607-2012; Wu, Dong/D-5375-2012 OI L'Ecuyer, Tristan/0000-0002-7584-4836; FU NASA [NNX07AR11G] FX This study was supported by NASA grant NNX07AR11G. NR 40 TC 258 Z9 266 U1 9 U2 45 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD DEC 10 PY 2008 VL 113 IS D23 AR D00A18 DI 10.1029/2008JD009982 PG 18 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 383JO UT WOS:000261670100004 ER PT J AU Taha, G Jaross, G Fussen, D Vanhellemont, F Kyrola, E McPeters, RD AF Taha, Ghassan Jaross, Glen Fussen, Didier Vanhellemont, Filip Kyroelae, Erkki McPeters, Richard D. TI Ozone profile retrieval from GOMOS limb scattering measurements SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID OSIRIS INSTRUMENT; ODIN SATELLITE; SAGE-II; SCIAMACHY; RADIATION; MISSION; ENVISAT AB We analyzed a set of Global Ozone Monitoring by Occultation of Stars (GOMOS) bright limb measurements with solar zenith angles less than 85 degrees and within 150 km of Stratospheric Aerosol and Gas Experiment II (SAGE II) measurements. In order to perform any species retrieval, GOMOS measurements were first corrected for stray light contamination. GOMOS pointing was analyzed using scene-based tangent height algorithms, and the best results were achieved using similar to 350 nm (Rayleigh) pixels that were consistent with GOMOS known accurate pointing. In order to demonstrate GOMOS bright limb capabilities, ozone profile retrievals were performed using GOMOS measurements of limb-scattered radiances with the Ozone Mapping and Profiler Suite limb profiler algorithm. The algorithm performs a simultaneous optimal estimation inversion of both Hartley-Huggins and Chappuis band radiances. We restricted our GOMOS ozone retrievals to the range 25-53 km, a region of relatively constant measurement uncertainty. In this first look at GOMOS limb data, the retrieved ozone profiles agree with collocated SAGE II measurements on average to within 10-15% and with a standard deviation of 10%. Retrieval results were consistent for both upper and lower GOMOS detector bands. C1 [Taha, Ghassan; Jaross, Glen] Sci Syst & Applicat Inc, Lanham, MD 20706 USA. [Fussen, Didier; Vanhellemont, Filip] Belgian Inst Space Aeron, B-1180 Brussels, Belgium. [Kyroelae, Erkki] Finnish Meteorol Inst, FIN-00101 Helsinki, Finland. [McPeters, Richard D.] NASA, Goddard Space Flight Ctr, Atmospheres Lab, Greenbelt, MD 20771 USA. RP Taha, G (reprint author), Sci Syst & Applicat Inc, Suite 500,10210 Greenbelt Rd, Lanham, MD 20706 USA. EM ghassan_taha@ssaihq.com; glen.jaross@nasa.gov; didier.fussen@aeronomie.be; filip.vanhellemont@aeronomie.be; erkki.kyrola@fmi.fi; richard.d.mcpeters@nasa.gov RI Kyrola, Erkki/E-1835-2014; McPeters, Richard/G-4955-2013 OI McPeters, Richard/0000-0002-8926-8462 NR 26 TC 8 Z9 8 U1 0 U2 0 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD DEC 10 PY 2008 VL 113 IS D23 AR D23307 DI 10.1029/2007JD009409 PG 15 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 383JO UT WOS:000261670100001 ER PT J AU Jeon, KJ Jeun, M Lee, E Lee, JM Lee, KI von Allmen, P Lee, A AF Jeon, Kye Jin Jeun, Minhong Lee, Eunsongyi Lee, Jun Min Lee, Kyoung-Il von Allmen, Paul Lee, Wooyoung TI Finite size effect on hydrogen gas sensing performance in single Pd nanowires SO NANOTECHNOLOGY LA English DT Article ID SENSOR; PERMEATION; MEMBRANES; SYSTEMS; ARRAYS AB We present the hydrogen sensing performance of individual Pd nanowires grown by electrodeposition into nanochannels of anodized aluminum oxide (AAO) templates investigated as a function of the nanowire diameter. Four-terminal devices based on individual Pd nanowires were found to successfully detect hydrogen gas (H(2)). Our experimental results show that the H2 sensing sensitivity increases and the response time decreases with decreasing diameter of Pd nanowires with d = 400, 200, 80 and 20 nm, due to the high surface-to-volume ratio and short diffusion paths, respectively. This is in qualitatively good agreement with simulated results obtained from a theoretical model based on a combination of the rate equation and diffusion equation. C1 [Jeon, Kye Jin; Jeun, Minhong; Lee, Eunsongyi; Lee, Jun Min; Lee, Kyoung-Il; Lee, Wooyoung] Yonsei Univ, Dept Mat Sci & Engn, Seoul 120749, South Korea. [von Allmen, Paul] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Lee, A (reprint author), Yonsei Univ, Dept Mat Sci & Engn, 134 Shinchon, Seoul 120749, South Korea. EM wooyoung@yonsei.ac.kr RI Lee, Eunsongyi/B-5162-2011 FU KOSEF [R15-2004024-00000-0]; Seoul Research and Business Development Program [10816]; Agency for Defense Development through the Defense Nano Technology Application Center FX This work was supported by KOSEF through the National Core Research Center for Nanomedical Technology (R15-2004024-00000-0), the Seoul Research and Business Development Program (10816) and the Agency for Defense Development through the Defense Nano Technology Application Center. NR 15 TC 27 Z9 28 U1 3 U2 17 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0957-4484 J9 NANOTECHNOLOGY JI Nanotechnology PD DEC 10 PY 2008 VL 19 IS 49 AR 495501 DI 10.1088/0957-4484/19/49/495501 PG 6 WC Nanoscience & Nanotechnology; Materials Science, Multidisciplinary; Physics, Applied SC Science & Technology - Other Topics; Materials Science; Physics GA 374KW UT WOS:000261043300014 PM 21730673 ER PT J AU Masse, M Le Mouelic, S Bourgeois, O Combe, JP Le Deit, L Sotin, C Bibring, JP Gondet, B Langevin, Y AF Masse, M. Le Mouelic, S. Bourgeois, O. Combe, J. -P. Le Deit, L. Sotin, C. Bibring, J. -P. Gondet, B. Langevin, Y. TI Mineralogical composition, structure, morphology, and geological history of Aram Chaos crater fill on Mars derived from OMEGA Mars Express data SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Article ID MERIDIANI-PLANUM; OPPORTUNITY ROVER; THERMAL INERTIA; HEMATITE; SURFACE; DEPOSITS; SPECTROMETER; EVOLUTION; SULFATES; TERRAINS AB Aram Chaos is a crater 280 km in diameter centered at 2.5 degrees N, 338.5 degrees E. It is filled by chaotic terrains overlain by a dome-shaped, layered 900 m thick formation displaying spectral signatures of ferric oxides on Thermal Emission Spectrometer (TES) and Observatoire pour la Mineralogie, L'Eau, les Glaces et L'Activite (OMEGA) medium spatial resolution data. We describe in detail the mineralogical composition, structure, and morphology of this crater fill using high-resolution data (OMEGA, Mars Orbiter Laser Altimeter, Mars Orbiter Camera, TES, Thermal Emission Imaging System, and High-Resolution Imaging Science Experiment). We infer the following formation scenario: the crater was first filled by a geological formation, the composition of which remains unclear because it is covered by dust. Widespread fracturing of this formation led to the development of chaotic terrains. Later, a second layered formation, presently dome shaped, was emplaced unconformably on the chaotic terrains. This younger unit is composed of a bright, poorly consolidated material that contains both monohydrated sulfates and ferric oxides according to OMEGA data. The surface of this formation is partially covered by dust and displays landforms indicating that the bright material has been mobilized by wind during or after its deposition. After its emplacement, this formation has been grooved down to various depths by large eolian erosion corridors. In these corridors, eolian removal of the bright material with a sulfate-rich matrix has left debris fans, sand sheets, and dunes, which display some of the strongest spectral signatures of ferric oxides on Mars. Similar residual deposits enriched in ferric oxides, overlying a layered formation containing both ferric oxides and sulfates, have been observed by the Opportunity rover in Meridiani Planum, suggesting a common formation process. C1 [Masse, M.; Le Mouelic, S.; Bourgeois, O.; Le Deit, L.] Univ Nantes, CNRS, UMR6112, Lab Planetol & Geodynam, F-44322 Nantes 3, France. [Bibring, J. -P.; Gondet, B.; Langevin, Y.] Univ Paris 11, Inst Astrophys Spatiale, F-91405 Orsay, France. [Combe, J. -P.] Bear Fight Ctr, Winthrop, WA 98862 USA. [Sotin, C.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Masse, M (reprint author), Univ Nantes, CNRS, UMR6112, Lab Planetol & Geodynam, 2 Chemin Houssiniere,BP 92205, F-44322 Nantes 3, France. EM marion.masse@univ-nantes.fr FU Centre National de la Recherche Scientifique; Institut National des Sciences de l'Univers; Centre National d'Etudes Spatiales; French government FX This work benefited from financial supports from the Centre National de la Recherche Scientifique, Institut National des Sciences de l'Univers (Programme National de Planetologie), and from the Centre National d'Etudes Spatiales. M. Masse is supported by a Ph. D. research grant from the French government (Ministere de l'Enseignement Superieur et de la Recherche). We thank W. H. Farrand and an anonymous reviewer for their insightful comments. Thorough advice from D. Mege, S. Pochat, and A. Bargery greatly improved the quality of this article. NR 57 TC 25 Z9 25 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 DEC 9 PY 2008 VL 113 IS E12 AR E12006 DI 10.1029/2008JE003131 PG 15 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 383QD UT WOS:000261687500002 ER PT J AU Huang, XC Schwenke, DW Lee, TJ AF Huang, Xinchuan Schwenke, David W. Lee, Timothy J. TI An accurate global potential energy surface, dipole moment surface, and rovibrational frequencies for NH(3) SO JOURNAL OF CHEMICAL PHYSICS LA English DT Article DE ab initio calculations; ammonia; correlation methods; coupled cluster calculations; excited states; functional analysis; molecular moments; perturbation theory; potential energy surfaces; rotational-vibrational states ID AB-INITIO; VARIATIONAL CALCULATIONS; PROJECTION OPERATORS; INTERSTELLAR AMMONIA; GIANT PLANETS; HOT AMMONIA; GLIESE 570D; FORCE-FIELD; EQUILIBRIUM; WATER AB A global potential energy surface (PES) that includes short and long range terms has been determined for the NH(3) molecule. The singles and doubles coupled-cluster method that includes a perturbational estimate of connected triple excitations and the internally contracted averaged coupled-pair functional electronic structure methods have been used in conjunction with very large correlation-consistent basis sets, including diffuse functions. Extrapolation to the one-particle basis set limit was performed and core correlation and scalar relativistic contributions were included directly, while the diagonal Born-Oppenheimer correction was added. Our best purely ab initio PES, denoted "mixed," is constructed from two PESs which differ in whether the ic-ACPF higher-order correlation correction was added or not. Rovibrational transition energies computed from the mixed PES agree well with experiment and the best previous theoretical studies, but most importantly the quality does not deteriorate even up to 10 300 cm(-1) above the zero-point energy (ZPE). The mixed PES was improved further by empirical refinement using the most reliable J=0-2 rovibrational transitions in the HITRAN 2004 database. Agreement between high-resolution experiment and rovibrational transition energies computed from our refined PES for J=0-6 is excellent. Indeed, the root mean square (rms) error for 13 HITRAN 2004 bands for J=0-2 is 0.023 cm(-1) and that for each band is always <= 0.06 cm(-1). For J=3-5 the rms error is always <= 0.15 cm(-1). This agreement means that transition energies computed with our refined PES should be useful in the assignment of new high-resolution NH(3) spectra and in correcting mistakes in previous assignments. Ideas for further improvements to our refined PES and for extension to other isotopolog are discussed. C1 [Huang, Xinchuan; Schwenke, David W.; Lee, Timothy J.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Schwenke, DW (reprint author), NASA, Ames Res Ctr, Mail Stop T27B-1, Moffett Field, CA 94035 USA. EM xinchuan.huang-1@nasa.gov; timothy.j.lee@nasa.gov; timothy.j.lee@nasa.gov RI HUANG, XINCHUAN/A-3266-2013; Lee, Timothy/K-2838-2012; schwenke, david/I-3564-2013 FU NASA; Spitzer Space Telescope GO program FX X. H. acknowledges the support by an appointment to the NASA Postdoctoral Program at the Ames Research Center, administered by Oak Ridge Associated Universities through a contract with NASA. Support from the Spitzer Space Telescope GO program (Cycle 4 ) is gratefully acknowledged. Professor Joel Bowman is thanked for insightful discussions and significant assistance in the early stages of this study. Helpful comments from Dr. Wesley Allen and encouragement from Dr. John Pearson and Dr. Mark Marley are gratefully acknowledged. NR 51 TC 43 Z9 43 U1 2 U2 20 PU AMER INST PHYSICS PI MELVILLE PA CIRCULATION & FULFILLMENT DIV, 2 HUNTINGTON QUADRANGLE, STE 1 N O 1, MELVILLE, NY 11747-4501 USA SN 0021-9606 J9 J CHEM PHYS JI J. Chem. Phys. PD DEC 7 PY 2008 VL 129 IS 21 AR 214304 DI 10.1063/1.3025885 PG 16 WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical SC Chemistry; Physics GA 379XW UT WOS:000261430900022 PM 19063558 ER PT J AU Russell, P Thomas, N Byrne, S Herkenhoff, K Fishbaugh, K Bridges, N Okubo, C Milazzo, M Daubar, I Hansen, C McEwen, A AF Russell, Patrick Thomas, Nicolas Byrne, Shane Herkenhoff, Kenneth Fishbaugh, Kathryn Bridges, Nathan Okubo, Chris Milazzo, Moses Daubar, Ingrid Hansen, Candice McEwen, Alfred TI Seasonally active frost-dust avalanches on a north polar scarp of Mars captured by HiRISE SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID REGION AB North-polar temporal monitoring by the High Resolution Imaging Science Experiment (HiRISE) orbiting Mars has discovered new, dramatic examples that Mars' CO2-dominated seasonal volatile cycle is not limited to quiet deposition and sublimation of frost. In early northern martian spring, 2008, HiRISE captured several cases of CO2 frost and dust cascading down a steep, polar scarp in discrete clouds. Analysis of morphology and process reveals these events to be similar to terrestrial powder avalanches, sluffs, and falls of loose, dry snow. Potential material sources and initiating mechanisms are discussed in the context of the Martian polar spring environment and of additional, active, aeolian processes observed on the plateau above the scarp. The scarp events are identified as a trigger for mass wasting of bright, fractured layers within the basal unit, and may indirectly influence the retreat rate of steep polar scarps in competing ways. Citation: Russell, P., et al. (2008), Seasonally active frost-dust avalanches on a north polar scarp of Mars captured by HiRISE, Geophys. Res. Lett., 35, L23204, doi: 10.1029/2008GL035790. C1 [Russell, Patrick; Thomas, Nicolas] Univ Bern, Inst Phys, Dept Space Res & Planetary Sci, CH-3012 Bern, Switzerland. [Bridges, Nathan; Hansen, Candice] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Daubar, Ingrid; McEwen, Alfred] Univ Arizona, Lunar & Planetary Lab, HiRISE Operat Ctr, Tucson, AZ 85721 USA. [Fishbaugh, Kathryn] Smithsonian Air & Space Museum, Ctr Earth & Planetary Studies, Washington, DC 20024 USA. [Herkenhoff, Kenneth; Okubo, Chris; Milazzo, Moses] US Geol Survey, Astrogeol Team, Flagstaff, AZ 86001 USA. RP Russell, P (reprint author), Univ Bern, Inst Phys, Dept Space Res & Planetary Sci, Sidlerstr 5, CH-3012 Bern, Switzerland. EM patrick.russell@space.unibe.ch; nicolas.thomas@space.unibe.ch; shane@lpl.arizona.edu; kherkenhoff@usgs.gov; fishbaughke@si.edu; nathan.t.bridges@jpl.nasa.gov; cokubo@usgs.gov; moses@usgs.gov; ingrid@pirl.lpl.arizona.edu; candice.j.hansen@jpl.nasa.gov; mcewen@pirl.lpl.arizona.edu RI Byrne, Shane/B-8104-2012; Daubar, Ingrid/N-1408-2013 FU Swiss National Science Foundation FX Thank you to P. Thomas and M. Koutnik for helpful reviews, the HiRISE and HiROC teams for help and discussions, and Sarah Mattson for jitter analysis. This work was supported in part by the Swiss National Science Foundation. NR 12 TC 16 Z9 16 U1 2 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 DEC 6 PY 2008 VL 35 IS 23 AR L23204 DI 10.1029/2008GL035790 PG 5 WC Geosciences, Multidisciplinary SC Geology GA 380NA UT WOS:000261471200004 ER PT J AU L'Ecuyer, TS Wood, NB Haladay, T Stephens, GL Stackhouse, PW AF L'Ecuyer, Tristan S. Wood, Norman B. Haladay, Taryn Stephens, Graeme L. Stackhouse, Paul W., Jr. TI Impact of clouds on atmospheric heating based on the R04 CloudSat fluxes and heating rates data set SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID EARTH RADIATION BUDGET; GENERAL-CIRCULATION MODEL; ISCCP DATA SETS; ENERGY BUDGET; CIRRUS CLOUDS; PART I; INTERANNUAL VARIATIONS; SEASONAL-VARIATION; AFRICAN CONTINENT; SOLAR IRRADIANCE AB Among the largest uncertainties in quantifying the radiative impacts of clouds are those that arise from the inherent difficulty in precisely specifying the vertical distribution of cloud optical properties using passive satellite measurements. Motivated by the need to address this problem, CloudSat was launched in April 2006 carrying into orbit the first millimeter wavelength cloud radar to be flown in space. Retrieved profiles of liquid and ice cloud microphysical properties from this Cloud Profiling Radar form the basis of the CloudSat's fluxes and heating rates algorithm, 2B-FLXHR, a standard product that provides high vertical resolution profiles of radiative fluxes and atmospheric heating rates on the global scale. This paper describes the physical basis of the 2B-FLXHR algorithm and documents the first year of 2B-FLXHR data in the context of assessing the radiative impact of clouds on global and regional scales. The analysis confirms that cloud contributions to atmospheric radiative heating are small on the global scale because of a cancelation of the much larger regional heating from high clouds in the tropics and cooling from low clouds at higher latitudes. Preliminary efforts to assess the accuracy of the 2B-FLXHR product using coincident CERES data demonstrate that outgoing longwave fluxes are better represented than those in the shortwave but both exhibit good agreement with CERES on scales longer than 5 days and larger than 5 degrees. Colocated CALIPSO observations of clouds that are undetected by CloudSat further indicate that while thin cirrus can introduce modest uncertainty in the products, low clouds that are obscured by ground clutter represent a far more important source of error in the current 2B-FLXHR product that must be addressed in subsequent versions of the algorithm. C1 [L'Ecuyer, Tristan S.; Wood, Norman B.; Haladay, Taryn; Stephens, Graeme L.] Colorado State Univ, Dept Atmospher Sci, Ft Collins, CO 80523 USA. [Stackhouse, Paul W., Jr.] NASA, Langley Res Ctr, Hampton, VA 23681 USA. RP L'Ecuyer, TS (reprint author), Colorado State Univ, Dept Atmospher Sci, Ft Collins, CO 80523 USA. EM tristan@atmos.colostate.edu RI L'Ecuyer, Tristan/C-7040-2013; L'Ecuyer, Tristan/E-5607-2012 OI L'Ecuyer, Tristan/0000-0002-7584-4836 FU NASA CloudSat Mission [NAS5-99237]; NASA Energy and Water [NAG06GC46G] FX This research was supported by NASA CloudSat Mission grant NAS5-99237 and NASA Energy and Water cycle Sponsored research (NEWS) grant NAG06GC46G. The authors thank the staff at the CloudSat Data Processing Center (DPC) and, in particular, Philip Partain for their assistance in implementing the FLXHR algorithm. All CloudSat data presented here were acquired through the DPC and can be accessed through their Web site http://www.cloudsat.cira.colostate.edu. The authors would also like to acknowledge Ed Eloranta and the University of Wisconsin Lidar Group (http://lidar.ssec.wisc.edu/) for graciously providing the AHSRL and MMCR data used in this study. NR 51 TC 67 Z9 68 U1 2 U2 21 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD DEC 6 PY 2008 VL 113 AR D00A15 DI 10.1029/2008JD009951 PG 15 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 380NN UT WOS:000261472500002 ER PT J AU Huang, D Liu, YG Wiscombe, W AF Huang, Dong Liu, Yangang Wiscombe, Warren TI Cloud tomography: Role of constraints and a new algorithm SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID INVERSION AB Retrieving spatial distributions of cloud liquid water content from limited-angle emission data (passive microwave cloud tomography) is ill-posed, and a small inaccuracy in the data and/or numerical treatments may result in a large error in the retrieval. Proper handling of the ill-posedness is an ongoing challenge to the atmospheric remote sensing community. In this paper we first analyze the major regularization methods that each apply a single but different constraint to their retrievals and extend these methods to allow for multiple constraints. We then develop a new iterative algorithm that can also incorporate complex physical constraints with great flexibility. To understand the influences of different constraints on the retrievals, we use the new iterative algorithm with various combinations of constraints to retrieve a stratocumulus cloud simulated with a large-eddy-simulation model. For this relatively homogeneous cloud case, the standard least squares method with no constraints, as expected, performs very poorly, and yields a very large retrieval error, making this method nearly useless. Adding a nonnegativity constraint reduces the mean retrieval error by a factor of 6 but the internal structure of the cloud is still not reproduced in the retrieval. Adding a smoothness constraint dramatically improves the retrieved spatial structure of the cloud, and brings the mean error down further, although the retrieved cloud top edges are still considerably blurred. Further adding the so-called double-side constraint (based on scaled adiabatic profiles) produces the best result; the retrieval faithfully reproduces the cloud water structure with a mean retrieval error of only one third of that of the nonnegativity and smoothness constrained method. C1 [Huang, Dong; Liu, Yangang; Wiscombe, Warren] Brookhaven Natl Lab, Dept Environm Sci, Upton, NY 11973 USA. [Wiscombe, Warren] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Huang, D (reprint author), Brookhaven Natl Lab, Dept Environm Sci, 75 Rutherford Dr, Upton, NY 11973 USA. EM dhuang@bnl.gov RI Liu, Yangang/H-6154-2011; Wiscombe, Warren/D-4665-2012; Huang, Dong/H-7318-2014 OI Wiscombe, Warren/0000-0001-6844-9849; Huang, Dong/0000-0001-9715-6922 NR 20 TC 5 Z9 7 U1 2 U2 6 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD DEC 5 PY 2008 VL 113 AR D23203 DI 10.1029/2008JD009952 PG 11 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 380NL UT WOS:000261472300004 ER PT J AU Lui, ATY Angelopoulos, V LeContel, O Frey, H Donovan, E Sibeck, DG Liu, W Auster, HU Larson, D Li, X Nose, M Fillingim, MO AF Lui, A. T. Y. Angelopoulos, V. LeContel, O. Frey, H. Donovan, E. Sibeck, D. G. Liu, W. Auster, H. U. Larson, D. Li, X. Nose, M. Fillingim, M. O. TI Determination of the substorm initiation region from a major conjunction interval of THEMIS satellites SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article ID EARTH PLASMA SHEET; MAGNETIC-FIELD OBSERVATIONS; THIN CURRENT SHEETS; BURSTY BULK FLOWS; BALLOONING INSTABILITY; CURRENT DISRUPTION; NEUTRAL LINE; PRESSURE-GRADIENT; AURORAL SUBSTORM; EXPANSION PHASE AB We investigate in detail the time history of substorm disturbances in the magnetotail observed during a major tail conjunction of Time History of Events and Macroscale Interactions during Substorms (THEMIS) satellites on 29 January 2008, 0700-0900 UT. During this interval, all THEMIS satellites were closely aligned along the tail axis near midnight and were bracketed in local time by GOES 11 and 12. The radial distance covered ranges from the geosynchronous altitude to similar to 30 R-E in the tail. This interval consists of three activations detected by the THEMIS satellites with good ground all-sky-camera observations of auroral activity. The first activation is a small substorm with spatially limited disturbance in the tail. The onset arc was equatorward of an undisturbed arc. The second activation is a moderate size substorm with the onset arc also being equatorward of an undisturbed arc. The third activation is an intensification of the substorm with its onset indicated by the second activation. The active auroral arc for this intensification was near the poleward boundary of the auroral oval. Analysis of these observations indicates that the first activation is a small substorm initiated in the near-Earth plasma sheet and does not involve magnetic reconnection of open magnetic field lines. Magnetic reconnection on closed field lines can be ruled out for this substorm because it cannot generate the observed high-speed plasma flow. The second and third activations are part of a moderate size substorm initiated also in the near-Earth plasma sheet, with a subsequent substorm intensification involving activity initiated tailward of similar to 30 R-E. Overall, the time history of substorm activity for these two substorms is consistent with the near-Earth initiation model. C1 [Lui, A. T. Y.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA. [Nose, M.] Kyoto Univ, Dept Geophys, Grad Sch Sci, Sakyo Ku, Kyoto 6068502, Japan. [Sibeck, D. G.] NASA, Goddard Space Flight Ctr, Laurel, MD 20723 USA. [Liu, W.; Li, X.] Univ Colorado, Atmospher & Space Phys Lab, Boulder, CO 80303 USA. [LeContel, O.] Ctr Etud Environm Terr & Planetaires, Inst Pierre Simon Laplace, F-78140 Velizy Villacoublay, France. [Frey, H.; Larson, D.; Fillingim, M. O.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Donovan, E.] Univ Calgary, Dept Phys & Astron, Calgary, AB T2N 1N4, Canada. [Auster, H. U.] Tech Univ Carolo Wilhelmina Braunschweig, Inst Geophys & Extraterr Phys, D-38106 Braunschweig, Germany. [Angelopoulos, V.] Univ Calif Los Angeles, Inst Geophys & Planetary Phys, Los Angeles, CA 90095 USA. RP Lui, ATY (reprint author), Johns Hopkins Univ, Appl Phys Lab, 11100 Johns Hopkins Rd, Laurel, MD 20723 USA. EM tony.lui@jhuapl.edu RI Sibeck, David/D-4424-2012; Liu, Wenlong/G-5585-2013; Nose, Masahito/B-1900-2015 OI Liu, Wenlong/0000-0001-7991-5067; Nose, Masahito/0000-0002-2789-3588 FU NASA [NAS5-02099, NNX07AU74G]; NSF [ATM-0630912]; German Zentrum fur Luft- und Raumfahrt [50QP0402] FX We thank J.P. McFadden, J.W. Bonnell, and H. Singer for availability of THEMIS ESA data, THEMIS EFI data, and GOES magnetometer data, respectively. This work was supported by the NASA contract NAS5-02099 to University of California, Berkeley, by the NSF grant ATM-0630912 and NASA grant NNX07AU74G to The Johns Hopkins University Applied Physics Laboratory, and by the German Ministerium fur Wirtschaft und Technologie and the German Zentrum fur Luft- und Raumfahrt under grant 50QP0402. NR 68 TC 34 Z9 34 U1 0 U2 11 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9380 J9 J GEOPHYS RES-SPACE JI J. Geophys. Res-Space Phys. PD DEC 5 PY 2008 VL 113 AR A00C04 DI 10.1029/2008JA013424 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 380PC UT WOS:000261476600001 ER PT J AU Lawson, JW Bauschlicher, CW Toulouse, J Filippi, C Umrigar, CJ AF Lawson, John W. Bauschlicher, Charles W., Jr. Toulouse, Julien Filippi, Claudia Umrigar, C. J. TI Quantum Monte Carlo study of the cooperative binding of NO(2) to fragment models of carbon nanotubes SO CHEMICAL PHYSICS LETTERS LA English DT Article ID CORRELATION-ENERGY; DENSITY; PSEUDOPOTENTIALS; EXCHANGE; ACCURATE AB Previous calculations on model systems for the cooperative binding of two NO(2) molecules to carbon nanotubes using density functional theory and second order Moller-Plesset perturbation theory gave results differing by 30 kcal/mol. Quantum Monte Carlo calculations are performed to study the role of electronic correlations in these systems and resolve the discrepancy between these previous calculations. Compared to QMC binding energies, MP2 and LDA are shown to overbind, while B3LYP and BPW91 underbind. PW91 gives the best agreement with QMC with a binding energy differing by only 3 kcal/mol. Basis set effects are also shown to be important. Published by Elsevier B. V. C1 [Lawson, John W.] NASA, Ames Res Ctr, Space Technol, Moffett Field, CA 94035 USA. [Toulouse, Julien] Univ Paris 06, Chim Theor Lab, Paris, France. [Toulouse, Julien] CNRS, Paris, France. [Filippi, Claudia] Leiden Univ, Inst Lorentz, NL-2300 RA Leiden, Netherlands. [Filippi, Claudia] Univ Twente, Fac Sci & Technol, NL-7500 AE Enschede, Netherlands. [Filippi, Claudia] Univ Twente, MESA Res Inst, NL-7500 AE Enschede, Netherlands. [Umrigar, C. J.] Cornell Univ, Atom & Solid State Phys Lab, Ithaca, NY 14853 USA. RP Lawson, JW (reprint author), NASA, Ames Res Ctr, Space Technol, Mail Stop 229-1, Moffett Field, CA 94035 USA. EM John.W.Lawson@nasa.gov RI Toulouse, Julien/A-1376-2010 FU NASA Ames DDF; European Marie Curie Outgoing International Fellowship [039750-QMC-DFT]; NSF; DOE FX J.W.L. and C. W. B. are civil servants in the TS Division ( Mail Stop 229-1). This work was funded in part by grants from the NASA Ames DDF, European Marie Curie Outgoing International Fellowship (039750-QMC-DFT), the NSF and the DOE. NR 29 TC 7 Z9 7 U1 0 U2 3 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0009-2614 J9 CHEM PHYS LETT JI Chem. Phys. Lett. PD DEC 4 PY 2008 VL 466 IS 4-6 BP 170 EP 175 DI 10.1016/j.cplett.2008.10.066 PG 6 WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical SC Chemistry; Physics GA 376LC UT WOS:000261184100014 ER PT J AU Zeng, N Yoon, JH Vintzileos, A Collatz, GJ Kalnay, E Mariotti, A Kumar, A Busalacchi, A Lord, S AF Zeng, Ning Yoon, Jin-Ho Vintzileos, Augustin Collatz, G. James Kalnay, Eugenia Mariotti, Annarita Kumar, Arun Busalacchi, Antonio Lord, Stephen TI Dynamical prediction of terrestrial ecosystems and the global carbon cycle: A 25-year hindcast experiment SO GLOBAL BIOGEOCHEMICAL CYCLES LA English DT Article ID NINO-SOUTHERN-OSCILLATION; EQUATORIAL PACIFIC; FORECAST SYSTEM; ATMOSPHERIC CO2; MODEL; SIMULATION; ENSO AB Using a 25-year hindcast experiment, we explore the possibility of seasonal-interannual prediction of terrestrial ecosystems and the global carbon cycle. This has been achieved using a prototype forecasting system in which the dynamic vegetation and terrestrial carbon cycle model VEGAS was forced with 15-member ensemble climate predictions generated by the NOAA/NCEP coupled climate forecasting system (CFS) for the period 1981-2005, with lead times up to 9 months. The results show that the predictability is dominated by the ENSO signal with its major influence on the tropical and subtropical regions, including South America, Indonesia, southern Africa, eastern Australia, western United States, and central Asia. There is also important non-ENSO related predictability such as that associated with midlatitude drought. Comparison of the dynamical prediction results with benchmark statistical prediction methods such as anomaly persistence and damping show that the dynamical method performs significantly better. The hindcasted ecosystem variables and carbon flux show significantly slower decrease in skill at longer lead time compared to the climate forcing variables, partly because of the memories in land and vegetation processes that filter out the higher-frequency noise and sustain the signal. C1 [Zeng, Ning; Yoon, Jin-Ho; Kalnay, Eugenia; Busalacchi, Antonio] Univ Maryland, Dept Atmospher & Ocean Sci, College Pk, MD 20742 USA. [Zeng, Ning; Mariotti, Annarita; Busalacchi, Antonio] Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20742 USA. [Collatz, G. James] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Kumar, Arun] NOAA, Climate Predict Ctr, Camp Springs, MD 20746 USA. [Vintzileos, Augustin; Lord, Stephen] NOAA, Environm Modeling Ctr, Camp Springs, MD 20746 USA. [Mariotti, Annarita] ENEA Casaccia, Rome, Italy. RP Zeng, N (reprint author), Univ Maryland, Dept Atmospher & Ocean Sci, College Pk, MD 20742 USA. EM zeng@atmos.umd.edu RI Kalnay, Eugenia/F-4393-2010; collatz, george/D-5381-2012; Zeng, Ning/A-3130-2008; YOON, JIN-HO/A-1672-2009; OI Zeng, Ning/0000-0002-7489-7629; YOON, JIN-HO/0000-0002-4939-8078; Kalnay, Eugenia/0000-0002-9984-9906 FU NOAA [NA04OAR4310091, NA04OAR4310114]; NSF [ATM0739677]; NASA [407191AG7] FX We thank S. Saha for discussion on CFS and NOAA/NCEP for making the CFS data available. Discussions with K. Mitchell and W. Higgins were helpful in improving our manuscript. The manuscript was significantly improved because of the comments from the Associate Editor Jim Randerson, Peter Rayner, and another anonymous reviewer. This research was supported by NOAA grants NA04OAR4310091 and NA04OAR4310114, NSF grant ATM0739677, and NASA grant 407191AG7. NR 32 TC 2 Z9 2 U1 0 U2 9 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0886-6236 EI 1944-9224 J9 GLOBAL BIOGEOCHEM CY JI Glob. Biogeochem. Cycle PD DEC 4 PY 2008 VL 22 IS 4 AR GB4015 DI 10.1029/2008GB003183 PG 13 WC Environmental Sciences; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Environmental Sciences & Ecology; Geology; Meteorology & Atmospheric Sciences GA 380MT UT WOS:000261470500003 ER PT J AU Sergienko, OV Bindschadler, RA Vornberger, PL MacAyeal, DR AF Sergienko, O. V. Bindschadler, R. A. Vornberger, P. L. MacAyeal, D. R. TI Ice stream basal conditions from block-wise surface data inversion and simple regression models of ice stream flow: Application to Bindschadler Ice Stream SO JOURNAL OF GEOPHYSICAL RESEARCH-EARTH SURFACE LA English DT Article ID WEST ANTARCTICA; BENEATH; SHEET AB [1] Widespread basal conditions controlling ice stream flows are still beyond the scope of direct observation, thus knowledge of their magnitudes and variabilities comes from inversion of surface measurements: ice velocities, surface elevations, and thicknesses. We present a new approach to implement a widely accepted inverse method on regular (10 x 10 km) blocks, smaller than the whole domain, to enhance the spatial resolution of calculated basal conditions. Inverted basal friction coefficients and calculated shear stress have sharp transitions and large variations in small areas. Overall, the obtained basal shear stress is very small in regions of fast flowing ice. The results of the inversion, along with the surface variables, are used to construct two simple regression models of Bindschadler Ice Stream ( former Ice Stream D) that reproduce 96% of observed velocity variations. While highly idealized, these regression models are sufficiently informative to be considered as parameterizations for ice stream flow in large-scale ice sheet models which lack the spatial and temporal resolution necessary to simulate ice stream dynamics in detail. C1 [Sergienko, O. V.] Portland State Univ, Dept Geol, Portland, OR 97207 USA. [Bindschadler, R. A.] NASA, Goddard Space Flight Ctr, Hydrospher & Biospher Sci Lab, Greenbelt, MD 20771 USA. [MacAyeal, D. R.] Univ Chicago, Dept Geophys Sci, Chicago, IL 60637 USA. [Vornberger, P. L.] Sci Applicat Int Corp, Beltsville, MD 20705 USA. RP Sergienko, OV (reprint author), Portland State Univ, Dept Geol, POB 751, Portland, OR 97207 USA. EM sergienk@pdx.edu OI MacAyeal, Douglas/0000-0003-0647-6176 FU NASA Postdoctoral Program at the Goddard Space Flight Center; Oak Ridge Associated Universities; NSF [OPP-0632168, OPP-0229546] FX We thank the associated editor, Shawn Marshall, Hilmar Gudmundsson, and anonymous reviewer for insightful comments and valuable suggestions that helped to improve the manuscript. O.V.S. was supported by an appointment to the NASA Postdoctoral Program at the Goddard Space Flight Center, administered by Oak Ridge Associated Universities through a contract with NASA, and by NSF grant OPP-0632168. D. R. M.' s participation was supported by NSF OPP- 0229546. NR 21 TC 11 Z9 11 U1 1 U2 5 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9003 EI 2169-9011 J9 J GEOPHYS RES-EARTH JI J. Geophys. Res.-Earth Surf. PD DEC 4 PY 2008 VL 113 IS F4 AR F04010 DI 10.1029/2008JF001004 PG 11 WC Geosciences, Multidisciplinary SC Geology GA 380OF UT WOS:000261474300001 ER PT J AU Konca, AO Avouac, JP Sladen, A Meltzner, AJ Sieh, K Fang, P Li, ZH Galetzka, J Genrich, J Chlieh, M Natawidjaja, DH Bock, Y Fielding, EJ Ji, C Helmberger, DV AF Konca, A. Ozgun Avouac, Jean-Philippe Sladen, Anthony Meltzner, Aron J. Sieh, Kerry Fang, Peng Li, Zhenhong Galetzka, John Genrich, Jeff Chlieh, Mohamed Natawidjaja, Danny H. Bock, Yehuda Fielding, Eric J. Ji, Chen Helmberger, Don V. TI Partial rupture of a locked patch of the Sumatra megathrust during the 2007 earthquake sequence SO NATURE LA English DT Article ID SUBDUCTION ZONE EARTHQUAKES; ANDAMAN EARTHQUAKE; DEFORMATION; ASPERITY; MODEL; SLIP AB The great Sumatra - Andaman earthquake and tsunami of 2004 was a dramatic reminder of the importance of understanding the seismic and tsunami hazards of subduction zones(1-4). In March 2005, the Sunda megathrust ruptured again, producing an event(5) of moment magnitude (M(w)) 8.6 south of the 2004 rupture area, which was the site of a similar event in 1861 (ref. 6). Concern was then focused on the Mentawai area, where large earthquakes had occurred in 1797 ( M(w) = 8.8) and 1833 (M(w) = 9.0)(6,7). Two earthquakes, one of M(w) = 8.4 and, twelve hours later, one of M(w) = 7.9, indeed occurred there on 12 September 2007. Here we show that these earthquakes ruptured only a fraction of the area ruptured in 1833 and consist of distinct asperities within a patch of the megathrust that had remained locked in the interseismic period. This indicates that the same portion of a megathrust can rupture in different patterns depending on whether asperities break as isolated seismic events or cooperate to produce a larger rupture. This variability probably arises from the influence of non- permanent barriers, zones with locally lower pre- stress due to the past earthquakes. The stress state of the portion of the Sunda megathrust that had ruptured in 1833 and 1797 was probably not adequate for the development of a single large rupture in 2007. Themoment released in 2007 amounts to only a fraction both of that released in 1833 and of the deficit of moment that had accumulated as a result of interseismic strain since 1833. The potential for a large megathrust event in the Mentawai area thus remains large. C1 [Konca, A. Ozgun; Avouac, Jean-Philippe; Sladen, Anthony; Meltzner, Aron J.; Sieh, Kerry; Galetzka, John; Genrich, Jeff; Natawidjaja, Danny H.; Helmberger, Don V.] CALTECH, Tecton Observ, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. [Fang, Peng; Bock, Yehuda] Univ Calif San Diego, Scripps Inst Oceanog, La Jolla, CA 92093 USA. [Li, Zhenhong] Univ Glasgow, COMET, Dept Geog & Earth Sci, Glasgow G12 8QQ, Lanark, Scotland. [Chlieh, Mohamed] Univ Nice Sophia Antipolis, Inst Rech Dev, Observ Cote Azur, F-06560 Valbonne, France. [Fielding, Eric J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Ji, Chen] Univ Calif Santa Barbara, Dept Geol Sci, Santa Barbara, CA 94106 USA. RP Avouac, JP (reprint author), CALTECH, Tecton Observ, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. EM avouac@gps.caltech.edu RI Meltzner, Aron/A-5585-2009; Li, Zhenhong/F-8705-2010; Avouac, Jean-Philippe/B-5699-2015; Fielding, Eric/A-1288-2007; Sladen, Anthony/A-2532-2017 OI Meltzner, Aron/0000-0002-2955-0896; Li, Zhenhong/0000-0002-8054-7449; Avouac, Jean-Philippe/0000-0002-3060-8442; Fielding, Eric/0000-0002-6648-8067; Sladen, Anthony/0000-0003-4126-0020 FU NSF [EAR-0538333]; Gordon and Betty Moore Foundation FX This study was partly funded by the NSF (grant EAR-0538333) and the Gordon and Betty Moore Foundation. This is Caltech Tectonics Observatory contribution no. 93. We thank R. Burgmann for comments and suggestions. NR 30 TC 141 Z9 145 U1 0 U2 27 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 0028-0836 J9 NATURE JI Nature PD DEC 4 PY 2008 VL 456 IS 7222 BP 631 EP 635 DI 10.1038/nature07572 PG 5 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 378QW UT WOS:000261340000039 PM 19052626 ER PT J AU Plante, I Cucinotta, FA AF Plante, Ianik Cucinotta, Francis A. TI Ionization and excitation cross sections for the interaction of HZE particles in liquid water and application to Monte Carlo simulation of radiation tracks SO NEW JOURNAL OF PHYSICS LA English DT Article ID ELECTRONS; RANGE; IONS AB Relativistic heavy ions of high charge (Z) and energy (E) (HZE) in galactic cosmic rays (GCR) are important contributors to space radiation risk because they cannot be shielded completely and their relative biological effectiveness is very high. To understand these risks, Monte Carlo track structure simulations by radiation transport codes are widely used in radiation biology to provide information on energy deposition and production of radiolytic species that damage cellular structures. In this paper, we show that relativistic corrections can be applied to existing semi-empirical cross section models for the ionization and excitation of water molecules by ions to extend the validity of their energy range up to similar to 10(4) MeV amu(-1). Similarly, an effective charge value correction is applied for Z > 2 ions. Simulations of HZE tracks have been performed by a new C++ Monte Carlo transport code, named RITRACKS, that uses these cross sections to calculate the stopping power, radial dose, XY-plane projections of track segments and radial distributions of primary radiolytic species (H-center dot, (OH)-O-center dot, H-2, H2O2 and e(aq)(-)) at similar to 10(-12) s. These new data will be useful to understand results from experiments performed at ion accelerators by discriminating the role of the so-called core and penumbra of the tracks. C1 [Plante, Ianik; Cucinotta, Francis A.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. [Plante, Ianik] Univ Space Res Assoc, Div Space Life Sci, Houston, TX 77058 USA. RP Plante, I (reprint author), NASA, Lyndon B Johnson Space Ctr, 2101 NASA Pkwy, Houston, TX 77058 USA. EM Ianik.Plante@USherbrooke.ca; Francis.A.Cucinotta@nasa.gov FU NASA Space Radiation Risk Assessment Project FX This research was supported by the NASA Space Radiation Risk Assessment Project. NR 21 TC 32 Z9 33 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 1367-2630 J9 NEW J PHYS JI New J. Phys. PD DEC 4 PY 2008 VL 10 AR 125020 DI 10.1088/1367-2630/10/12/125020 PG 15 WC Physics, Multidisciplinary SC Physics GA 380MQ UT WOS:000261470200004 ER PT J AU Palacios, C Zettler, E Amils, R Amaral-Zettler, L AF Palacios, Carmen Zettler, Erik Amils, Ricardo Amaral-Zettler, Linda TI Contrasting Microbial Community Assembly Hypotheses: A Reconciling Tale from the Rio Tinto SO PLOS ONE LA English DT Article ID EXTREME ACIDIC ENVIRONMENT; SPECIES RICHNESS; DIVERSITY; RIVER; ECOLOGY; SPAIN; BACTERIOPLANKTON; SEQUENCES; CHANCE; UNITS AB Background: The Rio Tinto (RT) is distinguished from other acid mine drainage systems by its natural and ancient origins. Microbial life from all three domains flourishes in this ecosystem, but bacteria dominate metabolic processes that perpetuate environmental extremes. While the patchy geochemistry of the RT likely influences the dynamics of bacterial populations, demonstrating which environmental variables shape microbial diversity and unveiling the mechanisms underlying observed patterns, remain major challenges in microbial ecology whose answers rely upon detailed assessments of community structures coupled with fine-scale measurements of physico-chemical parameters. Methodology/Principal Findings: By using high-throughput environmental tag sequencing we achieved saturation of richness estimators for the first time in the RT. We found that environmental factors dictate the distribution of the most abundant taxa in this system, but stochastic niche differentiation processes, such as mutation and dispersal, also contribute to observed diversity patterns. Conclusions/Significance: We predict that studies providing clues to the evolutionary and ecological processes underlying microbial distributions will reconcile the ongoing debate between the Baas Becking vs. Hubbell community assembly hypotheses. C1 [Palacios, Carmen; Amaral-Zettler, Linda] Josephine Bay Paul Ctr Comparat Mol Biol & Evolut, Marine Biol Lab, Woods Hole, MA USA. [Palacios, Carmen; Amaral-Zettler, Linda] NASA Astrobiol Inst, Marine Biol Lab, Woods Hole, MA USA. [Zettler, Erik; Amils, Ricardo] Univ Autonoma Madrid, Ctr Biol Mol, E-28049 Madrid, Spain. [Zettler, Erik] Sea Educ Assoc, Woods Hole, MA USA. [Amils, Ricardo] INTA CSIC, Ctr Astrobiol, Torrejon de Ardoz, Spain. RP Palacios, C (reprint author), Univ Perpignan Via Domitia, CNRS EPHE UPVD, UMR 5244, Ctr Biol & Ecol Trop & Mediterraneenne,Equipe Par, Perpignan, France. EM amaral@mbl.edu RI Palacios, Carmen/A-6255-2010 FU NASA Astrobiology Institute [NC-1054 LAZ]; Ministry of Science and Education [CGL2006/02534/BOS RA]; Spanish Centro de Astrobiologia FX This work was supported by grants from NASA Astrobiology Institute (NC-1054 LAZ) and from the Ministry of Science and Education (CGL2006/02534/BOS RA) and support to CP by the Spanish Centro de Astrobiologia. The funders had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript. NR 52 TC 24 Z9 24 U1 2 U2 18 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 DEC 4 PY 2008 VL 3 IS 12 AR e3853 DI 10.1371/journal.pone.0003853 PG 10 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 436YO UT WOS:000265452200006 PM 19052647 ER PT J AU Famiglietti, JS Ryu, D Berg, AA Rodell, M Jackson, TJ AF Famiglietti, James S. Ryu, Dongryeol Berg, Aaron A. Rodell, Matthew Jackson, Thomas J. TI Reply to comment by H. Vereecken et al. on "Field observations of soil moisture variability across scales" SO WATER RESOURCES RESEARCH LA English DT Editorial Material C1 [Famiglietti, James S.] Univ Calif Irvine, Dept Earth Syst Sci, Irvine, CA 92697 USA. [Berg, Aaron A.] Univ Guelph, Dept Geog, Guelph, ON N1G 2W1, Canada. [Ryu, Dongryeol; Jackson, Thomas J.] ARS, Hydrol & Remote Sensing Lab, USDA, Beltsville, MD 20705 USA. [Rodell, Matthew] NASA, Goddard Space Flight Ctr, Hydrol Sci Branch, Greenbelt, MD 20771 USA. RP Famiglietti, JS (reprint author), Univ Calif Irvine, Dept Earth Syst Sci, Irvine, CA 92697 USA. RI Rodell, Matthew/E-4946-2012; Ryu, Dongryeol/C-5903-2008 OI Rodell, Matthew/0000-0003-0106-7437; Ryu, Dongryeol/0000-0002-5335-6209 NR 6 TC 2 Z9 2 U1 1 U2 14 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0043-1397 J9 WATER RESOUR RES JI Water Resour. Res. PD DEC 4 PY 2008 VL 44 IS 12 AR W12602 DI 10.1029/2008WR007323 PG 2 WC Environmental Sciences; Limnology; Water Resources SC Environmental Sciences & Ecology; Marine & Freshwater Biology; Water Resources GA 380PV UT WOS:000261478500004 ER PT J AU Kuhlman, KR Venkat, P La Duc, MT Kuhlman, GM Mckay, CP AF Kuhlman, Kimberly R. Venkat, Parth La Duc, Myron T. Kuhlman, Gregory M. Mckay, Christopher P. TI Evidence of a microbial community associated with rock varnish at Yungay, Atacama Desert, Chile SO JOURNAL OF GEOPHYSICAL RESEARCH-BIOGEOSCIENCES LA English DT Review ID BIOLOGICAL SOIL CRUSTS; RIBOSOMAL-RNA ANALYSIS; PROJECT RDP-II; HYPERARID CORE; RADIOCARBON MEASUREMENTS; PHYLOGENETIC DIVERSITY; SUPEROXIDE-DISMUTASE; RADIATION-RESISTANCE; MICROCOLONIAL FUNGI; WHIPPLE MOUNTAINS AB Rock varnish is a very slow-growing nanostratigraphic coating consisting of approximately 70% fine-grained clay and 30% iron and manganese oxides that forms on the surfaces of rocks in arid and semiarid climates. The microbial diversity associated with rock varnish collected from the hyperarid Yungay region of the Atacama Desert was investigated using culture-independent biomolecular methods and an adenosine triphosphate (ATP) assay. The extraction of DNA from rock varnish collected at Yungay, a region in which little to no DNA has been extracted from the surface soil (<1 cm) to date, indicates that rock varnish may provide a niche habitat for microbial life where water is essentially absent. The clone library constructed suggests the presence of numerous phylogenetically distinct microorganisms, ranging in diversity from Cyanobacterial to a a-proteobacteria lineages. The findings also show that only a few micrometers of varnish material are enough to shelter microbes like Chroococcidiopsis spp. from the intense ultraviolet radiation present in the Atacama Desert. Whether or not microorganisms are involved in its nucleation and/or growth, rock varnish appears to provide a microhabitat resembling cryptoendolithic communities seen on a larger scale. C1 [Kuhlman, Kimberly R.] Planetary Sci Inst, Tucson, AZ 85719 USA. [Kuhlman, Gregory M.] Univ Wisconsin, Madison, WI 53706 USA. [La Duc, Myron T.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Mckay, Christopher P.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Venkat, Parth] CALTECH, Pasadena, CA 91106 USA. RP Kuhlman, KR (reprint author), Planetary Sci Inst, 1700 E Ft Lowell Rd,Suite 106, Tucson, AZ 85719 USA. EM kim@psi.edu; parthvenkat@gmail.com; myron.t.laduc@jpl.nasa.gov; gmkuhlman@wisc.edu; cmckay@arc.nasa.gov FU Jet Propulsion Laboratory's Director's Research and Development Fund (DRDF); NASA's Astrobiology Science and Technology Instrument Development (ASTID) Program FX We wish to thank Diana Northup, University of New Mexico, Ronald Crawford, University of Idaho, and Janice Strap, University of Ontario Institute of Technology, for constructive critical reviews of this work. We also wish to thank Tanzhou Liu for his artful fabrication and imaging of ultra-thin petrographic thin sections of rock varnish from Yungay. This work was funded by the Jet Propulsion Laboratory's Director's Research and Development Fund (DRDF) and by NASA's Astrobiology Science and Technology Instrument Development (ASTID) Program. NR 119 TC 19 Z9 19 U1 1 U2 26 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0148-0227 J9 J GEOPHYS RES-BIOGEO JI J. Geophys. Res.-Biogeosci. PD DEC 3 PY 2008 VL 113 IS G4 AR G04022 DI 10.1029/2007JG000677 PG 14 WC Environmental Sciences; Geosciences, Multidisciplinary SC Environmental Sciences & Ecology; Geology GA 380NW UT WOS:000261473400001 ER PT J AU Galli, A Fok, MC Wurz, P Barabash, S Grigoriev, A Futaana, Y Holmstrom, M Ekenback, A Kallio, E Gunell, H AF Galli, A. Fok, M. -C. Wurz, P. Barabash, S. Grigoriev, A. Futaana, Y. Holmstroem, M. Ekenbaeck, A. Kallio, E. Gunell, H. TI Tailward flow of energetic neutral atoms observed at Venus SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Article ID 1ST-ENA OBSERVATIONS; UPPER-ATMOSPHERE; MARS; HYDROGEN; ASPERA-4; OXYGEN AB The Analyzer of Space Plasma and Energetic Atoms (ASPERA-4) experiment on Venus Express provides the first measurements of energetic neutral atoms (ENAs) from Venus. The results improve our knowledge on the interaction of the solar wind with a nonmagnetized planet and they present an observational constraint to existing plasma models. We characterize the tailward flow of hydrogen ENAs observed on the nightside by providing global images of the ENA intensity. The images show a highly concentrated tailward flow of hydrogen ENAs tangential to the Venus limb around the Sun's direction. No oxygen ENAs above the instrument threshold are detected. The observed ENA intensities are reproduced with a simple ENA model within a factor of 2, indicating that the observed hydrogen ENAs originate from shocked solar wind protons that charge exchange with the neutral hydrogen exosphere. C1 [Galli, A.; Wurz, P.] Univ Bern, Inst Phys, CH-3012 Bern, Switzerland. [Fok, M. -C.] NASA, Goddard Space Flight Ctr, Geospace Phys Lab, Greenbelt, MD 20771 USA. [Gunell, H.] W Virginia Univ, Dept Phys, Morgantown, WV 26506 USA. [Kallio, E.] Finnish Meteorol Inst, FIN-00101 Helsinki, Finland. [Barabash, S.; Grigoriev, A.; Futaana, Y.; Holmstroem, M.; Ekenbaeck, A.] Inst Rymdfys, Kiruna, Sweden. RP Galli, A (reprint author), Univ Bern, Inst Phys, Sidlerstr 5, CH-3012 Bern, Switzerland. EM wurz@space.unibe.ch RI Fok, Mei-Ching/D-1626-2012; Gunell, Herbert/D-5611-2013; Kallio, Esa/F-9410-2014; OI Kallio, Esa/0000-0002-9791-804X; Gunell, Herbert/0000-0001-5379-1158 FU Swiss National Science Foundation FX The ASPERA-4 experiment on the ESA Venus Express mission is a joint effort between 16 laboratories in 11 countries, all sponsored by their national agencies. We thank all these agencies as well as the various departments/institutes hosting these efforts. The lead author wishes to acknowledge the support of the Swiss National Science Foundation. NR 25 TC 12 Z9 13 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 DEC 2 PY 2008 VL 113 AR E00B15 DI 10.1029/2008JE003096 PG 17 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 380OM UT WOS:000261475000001 ER PT J AU Teanby, NA de Kok, R Irwin, PGJ Osprey, S Vinatier, S Gierasch, PJ Read, PL Flasar, FM Conrath, BJ Achterberg, RK Bezard, B Nixon, CA Calcutt, SB AF Teanby, N. A. de Kok, R. Irwin, P. G. J. Osprey, S. Vinatier, S. Gierasch, P. J. Read, P. L. Flasar, F. M. Conrath, B. J. Achterberg, R. K. Bezard, B. Nixon, C. A. Calcutt, S. B. TI Titan's winter polar vortex structure revealed by chemical tracers SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Article ID COMPOSITE INFRARED SPECTROMETER; GENERAL-CIRCULATION MODEL; MIDDLE ATMOSPHERE; MERIDIONAL CIRCULATION; POTENTIAL-VORTICITY; RADIATIVE-TRANSFER; CASSINI/CIRS DATA; GRAVITY-WAVES; STRATOSPHERE; DYNAMICS AB The winter polar vortex on Saturn's largest moon Titan has profound effects on atmospheric circulation and chemistry and for the current northern midwinter season is the major dynamical feature of Titan's stratosphere and mesosphere. We use 2 years of observations from Cassini's composite infrared spectrometer to determine cross sections of five independent chemical tracers (HCN, HC3N, C2H2, C3H4, and C4H2), which are then used to probe dynamical processes occurring within the vortex. Our results provide compelling evidence that the vortex acts as a strong mixing barrier in the stratosphere and mesosphere, effectively separating a tracer-enriched air mass in the north from air at lower latitudes. In the mesosphere, above the level of the vortex jet, a tracer-depleted zone extends away from the north pole toward the equator and enrichment is confined to high northern latitudes. However, below this level, mixing processes cause tongues of gas to extend away from the polar region toward the equator. These features are not reproduced by current general circulation models and suggest that a residual polar circulation is present and that waves and instabilities form a more important part of Titan's atmospheric dynamics than previously thought. We also observe an unexpected enrichment of C4H2 in the northern stratosphere, which suggests photochemical polymerization of C2H2. Our observations provide stringent new constraints for dynamical and photochemical models and identify key polar processes for the first time. Some of the processes we see have analogues in Earth's polar vortex, while others are unique to Titan. C1 [de Kok, R.; Irwin, P. G. J.; Osprey, S.; Read, P. L.; Calcutt, S. B.] Univ Oxford, Oxford OX1 3PU, England. [Achterberg, R. K.; Nixon, C. A.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Vinatier, S.; Bezard, B.] Observ Paris, LESIA, F-92195 Meudon, France. [Gierasch, P. J.; Conrath, B. J.] Cornell Univ, Dept Astron, Ithaca, NY 14853 USA. [Flasar, F. M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Teanby, NA (reprint author), Univ Oxford, Oxford OX1 3PU, England. EM teanby@atm.ox.ac.uk RI Nixon, Conor/A-8531-2009; Flasar, F Michael/C-8509-2012; Osprey, Scott/P-6621-2016; OI Nixon, Conor/0000-0001-9540-9121; Osprey, Scott/0000-0002-8751-1211; Calcutt, Simon/0000-0002-0102-3170; Teanby, Nicholas/0000-0003-3108-5775; Irwin, Patrick/0000-0002-6772-384X FU UK Science and Technology Facilities Council FX This research was funded by the UK Science and Technology Facilities Council. The authors would like to thank the Cassini-CIRS instrument team, without which this research would not have been possible. We also thank Bryan Lawrence at the British Atmospheric Data Centre for supplying the gravity wave parameterization code. NR 59 TC 33 Z9 33 U1 0 U2 6 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 DEC 2 PY 2008 VL 113 IS E12 AR E12003 DI 10.1029/2008JE003218 PG 13 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 380OO UT WOS:000261475200003 ER PT J AU Soares, MCR Rabiu, AB Gopalswamy, N Thompson, BJ Davila, JM Sobrinho, AA AF Soares, M. C. Rabello Rabiu, A. B. Gopalswamy, N. Thompson, B. J. Davila, J. M. Sobrinho, A. A. TI Outreach activities during the 2006 total solar eclipse sponsored by the International Heliophysical Year SO ADVANCES IN SPACE RESEARCH LA English DT Article DE Solar eclipse; Education; Sun; Solar-terrestrial relations; Solar system; Africa; Asia; South America AB The International Heliophysical Year (IHY) is an international program of scientific research to advance our understanding of the physical processes that govern the Sun, Earth and heliosphere. It has a strong educational component, linking research and education. Here, we describe the outreach activities during the 2006 total solar eclipse sponsored by IHY. (C) 2007 COSPAR. Published by Elsevier Ltd. All rights reserved. C1 [Soares, M. C. Rabello] Stanford Univ, HEPL Solar Phys, Stanford, CA 94305 USA. [Rabiu, A. B.] Fed Univ Technol Akure, Dept Phys, Akure, Nigeria. [Gopalswamy, N.; Thompson, B. J.; Davila, J. M.] NASA, Goddard Space Flight Ctr, Lab Solar & Space Phys, Solar Phys Branch, Greenbelt, MD 20771 USA. [Sobrinho, A. A.] Ctr Fed Educ Tecnol Rio Grande do Norte, Natal, RN, Brazil. RP Soares, MCR (reprint author), Stanford Univ, HEPL Solar Phys, 445 Via Palou, Stanford, CA 94305 USA. EM csoares@sun.stanford.edu; tunderabiu@yahoo.com; antonioaraujo@cefetrn.br RI Gopalswamy, Nat/D-3659-2012; Thompson, Barbara/C-9429-2012; OI Rabello Soares, Maria Cristina/0000-0003-0172-3713 NR 11 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 0273-1177 J9 ADV SPACE RES JI Adv. Space Res. PD DEC 1 PY 2008 VL 42 IS 11 BP 1792 EP 1799 DI 10.1016/j.asr.2007.04.014 PG 8 WC Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences GA 381NP UT WOS:000261543500003 ER PT J AU Mitchell, SE Drobnes, E Colina-Trujillo, MS Noel-Storr, J AF Mitchell, Sara E. Drobnes, Emilie Colina-Trujillo, M. Sol Noel-Storr, Jacob TI NASA Family Science Night: Changing perceptions one family at a time SO ADVANCES IN SPACE RESEARCH LA English DT Article DE Family; Science; Parents; Parental involvement; Out-of-school; Perceptions; Engagement; Middle school; Informal education AB Parents and families have the greatest influence on children's attitudes towards education and career choices. If students' attitudes towards science, particularly the physical sciences, are not influenced positively by parental/familial attitudes, efforts to improve the quality of content and teaching of these subjects in school may be futile. Research shows that parental involvement increases student achievement outcomes, and family-oriented programs have a direct impact on student performance. Based on this premise, the NASA Goddard Space Flight Center started a series of Family Science Nights for middle school students and their families. The program provides a non-threatening venue for families to explore the importance of science and technology in our daily lives by engaging in learning activities that change their perception and understanding of science - making it more practical and approachable for participants of all ages. Family Science Night strives to change the way that students and their families participate in science, within the program and beyond. (C) 2003 COSPAR. Published by Elsevier Ltd. All rights reserved. C1 [Mitchell, Sara E.] NASA, Goddard Space Flight Ctr, SP Syst & Astrophys Sci Div, Greenbelt, MD 20771 USA. [Drobnes, Emilie; Colina-Trujillo, M. Sol] NASA, Goddard Space Flight Ctr, ADNET & Heliophys Sci Div, Greenbelt, MD 20771 USA. [Noel-Storr, Jacob] Rochester Inst Technol, Ctr Imaging Sci, Rochester, NY 14623 USA. RP Mitchell, SE (reprint author), NASA, Goddard Space Flight Ctr, SP Syst & Astrophys Sci Div, Code 660-1, Greenbelt, MD 20771 USA. EM sara.mitchell@nasa.gov; emilie.drob-nes@nasa.gov; mcolina@pop400.gsfc.nasa.gov; jake@cis.rit.edu NR 5 TC 0 Z9 0 U1 2 U2 7 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 0273-1177 J9 ADV SPACE RES JI Adv. Space Res. PD DEC 1 PY 2008 VL 42 IS 11 BP 1844 EP 1847 DI 10.1016/j.asr.2008.01.004 PG 4 WC Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences GA 381NP UT WOS:000261543500010 ER PT J AU Beck-Winchatz, B Riccobono, MA AF Beck-Winchatz, Bernhard Riccobono, Mark A. TI Advancing participation of blind students in Science, Technology, Engineering, and Math SO ADVANCES IN SPACE RESEARCH LA English DT Article DE Science education; Special needs; Diversity; Blindness AB Like their sighted peers, many blind students in elementary, middle, and high school are naturally interested in space. This interest can motivate them to learn fundamental scientific, quantitative, and critical thinking skills, and sometimes even lead to careers in Science, Technology, Engineering, and Math (STEM) disciplines. However, these students are often at a disadvantage in science because of the ubiquity of important graphical information that is generally not available in accessible formats, the unfamiliarity of teachers with non-visual teaching methods, lack of access to blind role models, and the low expectations of their teachers and parents. We discuss joint efforts by the National Aeronautics and Space Administration (NASA) and the National Federation of the Blind's (NFB) National Center for Blind Youth in Science (NCBYS) to develop and implement strategies to promote opportunities for blind youth in science. These include the development of tactile space science books and curriculum materials, science academies for blind middle school and high school students, and college-level internship and mentoring programs. The partnership with the NFB exemplifies the effectiveness of collaborations between NASA and consumer-directed organizations to improve opportunities for underserved and underrepresented individuals. (C) 2007 COSPAR. Published by Elsevier Ltd. All rights reserved. C1 [Beck-Winchatz, Bernhard] De Paul Univ, NASA, SMD Broker Facilitator Program, Chicago, IL 60614 USA. [Riccobono, Mark A.] Jernigan Inst, Baltimore, MD 21230 USA. RP Beck-Winchatz, B (reprint author), De Paul Univ, NASA, SMD Broker Facilitator Program, 990 Fullerton,Suite 4400, Chicago, IL 60614 USA. EM bbeckwin@depaul.edu RI Duello, Theresa/P-5752-2015 NR 17 TC 9 Z9 9 U1 1 U2 23 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 0273-1177 J9 ADV SPACE RES JI Adv. Space Res. PD DEC 1 PY 2008 VL 42 IS 11 BP 1855 EP 1858 DI 10.1016/j.asr.2007.05.080 PG 4 WC Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences GA 381NP UT WOS:000261543500012 ER PT J AU Bering, EA Bacon, L Copper, KK Hansen, LJ Sanchez, MJ AF Bering, E. A., III Bacon, L. Copper, K. K. Hansen, L. J. Sanchez, M. J. TI The American Institute of Aeronautics and Astronautics pre-college outreach program SO ADVANCES IN SPACE RESEARCH LA English DT Article DE Education; Pre-college; National program ID ASPIRATIONS; STUDENTS; ATTITUDE; SCIENCE; ADOLESCENTS; SCHOOL; FAMILY AB Many United States, school children perceive science, technology, engineering, and mathematics (STEM) as difficult, boring and often irrelevant subjects. The possible reasons for this problem are endlessly debated. However, the economic, social, and overall national importance of producing graduates who are technically literate and enthusiastic in their support of a rational scientific world is essential to our nation. This apparent STEM crisis should motivate the many scientific and engineering societies to develop STEM outreach programs aimed at students, parents, teachers and schools (grades K-12). The American Institute of Aeronautics and Astronautics (AIAA) is among those organizations that have identified the need to educate students and teachers about STEM current events and their direct effects on the United States population in a way that motivates both. The AIAA has established a pre-college outreach program that has several major elements that will be described in this paper. Elements focused on the teachers include a pre-college Educator Associate Membership program, classroom grants to support hands-on learning activities, Educator of the Year awards and recognition program and two national workshop events. The first workshop event, Passport to the Future, is held annually in conjunction with the Joint Propulsion Conference. It is intended to provide summertime training in Aerospace science education to classroom teachers, in conjunction with a national professional conference. The second workshop, Education Alley, is held in the fall in conjunction with the "Space" series of conferences. This program is aimed at direct outreach to local students in the conference host city, providing fun, interesting, and educational events that promote STEM. The AIAA also encourages and supports pre-college outreach activities sponsored by the local AIAA sections through leadership training, activity and material support. (C) 2007 COSPAR. Published by Elsevier Ltd. All rights reserved. C1 [Bering, E. A., III] Univ Houston, Dept Phys, Houston, TX 77204 USA. [Bering, E. A., III] Univ Houston, Dept Elect & Comp Engn, Houston, TX 77204 USA. [Bacon, L.] Amer Inst Aeronaut & Astronaut, Reston, VA 20191 USA. [Copper, K. K.] IDS, Boeing, Ofallon, MO 63366 USA. [Hansen, L. J.] HRP Syst Inc, Torrance, CA 90503 USA. [Sanchez, M. J.] NASA, Johnson Space Ctr, Houston, TX 77058 USA. RP Bering, EA (reprint author), Univ Houston, Dept Phys, 617 Sci & Res Bldg 1, Houston, TX 77204 USA. EM eabering@uh.edu; lisab@aiaa.org; karen.k.copper@boeing.com; hansen@hrpsystems.com; merri.j.sanchez@nasa.gov NR 16 TC 0 Z9 0 U1 1 U2 5 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 0273-1177 J9 ADV SPACE RES JI Adv. Space Res. PD DEC 1 PY 2008 VL 42 IS 11 BP 1869 EP 1878 DI 10.1016/j.asr.2007.11.009 PG 10 WC Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences GA 381NP UT WOS:000261543500015 ER PT J AU Thomas, JL Diskin, B Rumsey, CL AF Thomas, James L. Diskin, Boris Rumsey, Christopher L. TI Toward Verification of Unstructured-Grid Solvers SO AIAA JOURNAL LA English DT Article; Proceedings Paper CT AIAA 46th Aerospace Sciences Meeting and Exhibit CY JAN 07-10, 2008 CL Reno, NV SP Amer Inst Aeronaut & Astronaut ID NONUNIFORM MESHES; SCHEMES; ACCURACY; FLOWS AB New methodology for verification of finite volume computational methods using unstructured grids is presented. The discretization-order properties are studied in computational windows, easily constructed within a collection of grids or a single grid. Tests are performed within each window and address a combination of problem-, solution-, and discretization/grid-related features affecting discretization-error convergence. The windows can be adjusted to isolate particular elements of the computational scheme, such as the interior discretization, the boundary discretization, or singularities. Studies can use traditional grid-refinement computations within a fixed window or downscaling, a recently introduced technique in which computations are made within windows contracting toward a focal point of interest. Grids within the windows are constrained to be consistently refined, allowing a meaningful assessment of asymptotic error convergence on unstructured grids. Demonstrations of the method are shown, including a comparative accuracy assessment of commonly used schemes on general mixed grids and the identification of local accuracy deterioration at boundary intersections. Recommendations to enable attainment of design-order discretization errors for large-scale computational simulations are given. C1 [Thomas, James L.; Rumsey, Christopher L.] NASA, Langley Res Ctr, Computat Aerosci Branch, Hampton, VA 23681 USA. [Diskin, Boris] Natl Inst Aerosp, Hampton, VA 23666 USA. RP Thomas, JL (reprint author), NASA, Langley Res Ctr, Computat Aerosci Branch, Mail Stop 128, Hampton, VA 23681 USA. EM James.L.Thomas@nasa.gov; bdiskin@nianet.org; c.l.rumsey@nasa.gov NR 24 TC 16 Z9 16 U1 2 U2 2 PU AMER INST AERONAUT ASTRONAUT PI RESTON PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA SN 0001-1452 J9 AIAA J JI AIAA J. PD DEC PY 2008 VL 46 IS 12 BP 3070 EP 3079 DI 10.2514/1.36655 PG 10 WC Engineering, Aerospace SC Engineering GA 381IA UT WOS:000261528000008 ER PT J AU Nichols, RH Tramel, RW Buning, PG AF Nichols, Robert H. Tramel, Robert W. Buning, Pieter G. TI Evaluation of Two High-Order Weighted Essentially Nonoscillatory Schemes SO AIAA JOURNAL LA English DT Article; Proceedings Paper CT AIAA 25th Applied Aerodynamics Conference CY JUN 25-28, 2007 CL Miami, FL SP Amer Inst Aeronaut & Astronaut ID EFFICIENT IMPLEMENTATION; CONSERVATION-LAWS; COMPUTATIONS; CYLINDER; FLOWS; GRIDS; FORM AB Two fifth-order spatial weighted essentially nonoscillatory schemes for the convective terms were added to the OVERFLOW 2 implicit overset Navier-Stokes flow solver. The method used to incorporate the schemes is similar to a monotone upstream-centered scheme for conservation laws and requires no modification of the viscous terms, transport equations, or turbulence models in the code. The new flux calculation schemes were applied to problems involving vortex convection, strong shocks, and large scale unsteady flows. The weighted essentially nonoscillatory schemes were found to have much lower numerical dissipation/dispersion than traditional third-order spatial monotone upstream-centered schemes for conservation laws. Both weighted essentially nonoscillatory schemes were numerically robust over a wide range of Mach numbers when solved using the existing implicit schemes within OVERFLOW 2. The weighted essentially nonoscillatory schemes also provided improved numerical accuracy over traditional third-order spatial monotone upstream-centered schemes for conservation laws on the same computational grid for all the applications examined here. The weighted essentially nonoscillatory schemes are 10-30% more expensive than the third-order spatial monotone upstream-centered schemes for conservation laws depending on choice of implicit solver. C1 [Nichols, Robert H.] Univ Alabama Birmingham, Dept Mech Engn, Birmingham, AL 35294 USA. [Tramel, Robert W.] Digital Fus Inc, Huntsville, AL 35806 USA. [Buning, Pieter G.] NASA, Langley Res Ctr, Configurat Aerodynam Branch, Hampton, VA 23681 USA. RP Nichols, RH (reprint author), Univ Alabama Birmingham, Dept Mech Engn, Birmingham, AL 35294 USA. NR 34 TC 10 Z9 13 U1 0 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 DEC PY 2008 VL 46 IS 12 BP 3090 EP 3102 DI 10.2514/1.36849 PG 13 WC Engineering, Aerospace SC Engineering GA 381IA UT WOS:000261528000010 ER PT J AU Kojima, J Nguyen, QV AF Kojima, Jun Nguyen, Quang-Viet TI Observation of Turbulent Mixing in Lean-Direct-Injection Combustion at Elevated Pressure SO AIAA JOURNAL LA English DT Article ID SPONTANEOUS RAMAN-SCATTERING; LARGE-EDDY SIMULATION; TURBINE MODEL COMBUSTOR; SIMULTANEOUS TEMPERATURE; HYDROCARBON FLAMES; LASER DIAGNOSTICS; DIFFUSION FLAME; SWIRL FLAMES; GAS; SPECTROSCOPY AB We report the first quantitative single-shot multiscalar data obtained from a realistic air-fed lean-direct-injection burner operating on gaseous methane (CH(4)) fuel at elevated pressure (5 atm) using single-shot spontaneous Raman spectroscopy. From a statistical analysis of the multiscalar data, we present spatially mapped probability density functions of the concentration of CH(4) and O(2), and the instantaneous temperature. The measured three-scalar correlations and probability density functions provide insights into the nature and extent of the mixing process and its impact on the subsequent combustion process. The data will also be useful for comparison with the various turbulence-chemistry interaction models such as large-eddy simulation. The swirl-stabilized flame investigated in this paper was characterized as operating in a partially premixed combustion regime that was dominated by turbulent mixing provided by the lean-direct-injection configuration. Although a majority of the single-shot data indicated complete or near-complete reactions including stoichiometric combustion, a considerable number of the data points exhibited incomplete combustion characterized by a substantial amount of residual fuel at intermediate temperatures or were simply unreacted with little or no preheating of the mixture. C1 [Kojima, Jun] Ohio Aerosp Inst, Turbomachinery & Prop Syst Team, Cleveland, OH 44142 USA. [Nguyen, Quang-Viet] NASA, John H Glenn Res Ctr Lewis Field, Combust Branch, Cleveland, OH 44135 USA. RP Kojima, J (reprint author), Ohio Aerosp Inst, Turbomachinery & Prop Syst Team, Cleveland, OH 44142 USA. FU NASA FX The authors acknowledge financial support by the Supersonics program and the Subsonic Fixed Wing program under Fundamental Aeronautics at NASA John H. Glenn Research Center at Lewis Field. The authors also acknowledge Gregg Calhoun for his assistance in the operation of the facilities. NR 51 TC 6 Z9 6 U1 1 U2 7 PU AMER INST AERONAUT ASTRONAUT PI RESTON PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA SN 0001-1452 J9 AIAA J JI AIAA J. PD DEC PY 2008 VL 46 IS 12 BP 3116 EP 3127 DI 10.2514/1.37433 PG 12 WC Engineering, Aerospace SC Engineering GA 381IA UT WOS:000261528000012 ER PT J AU Yung, PT Ponce, A AF Yung, Pun To Ponce, Adrian TI Fast Sterility Assessment by Germinable-Endospore Biodosimetry SO APPLIED AND ENVIRONMENTAL MICROBIOLOGY LA English DT Article ID BACTERIAL-SPORES; MEDICAL DEVICES; INACTIVATION; RESISTANCE; MODEL AB The increased demand for sterile products has created the need for rapid technologies capable of validating the hygiene of industrial production processes. Bacillus endospores are in standard use as biological indicators for evaluating the effectiveness of sterilization processes. Currently, culture-based methods, requiring more than 2 days before results become available, are employed to verify endospore inactivation. We describe a rapid, microscopy-based endospore viability assay (mu EVA) capable of enumerating germinable endospores in less than 15 min. mu EVA employs time-gated luminescence microscopy to enumerate single germinable endospores via terbium-dipicolinate (Tb-DPA) luminescence, which is triggered under UV excitation as 10(8) DPA molecules are released during germination on agarose containing Tb(3+) and a germinant (e. g., L-alanine). Inactivation of endospore populations to sterility was monitored with mu EVA as a function of thermal and UV dosage. A comparison of culturing results yielded nearly identical decimal reduction values, thus validating mu EVA as a rapid biodosimetry method for monitoring sterilization processes. The simple Tb-DPA chemical test for germinability is envisioned to enable fully automated instrumentation for in-line monitoring of hygiene in industrial production processes. C1 [Yung, Pun To; Ponce, Adrian] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Ponce, A (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM adrian.ponce@jpl.nasa.gov FU NASA; National Aeronautic and Space Administration; NASA's Astrobiology and Planetary Protection Programs; Department of Homeland Security's Chemical and Biological Research & Development Program FX P. T. Y. acknowledges support from the NASA postdoctoral program. The research described in this paper was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautic and Space Administration and was sponsored by NASA's Astrobiology and Planetary Protection Programs and by the Department of Homeland Security's Chemical and Biological Research & Development Program. NR 32 TC 18 Z9 18 U1 0 U2 8 PU AMER SOC MICROBIOLOGY PI WASHINGTON PA 1752 N ST NW, WASHINGTON, DC 20036-2904 USA SN 0099-2240 J9 APPL ENVIRON MICROB JI Appl. Environ. Microbiol. PD DEC PY 2008 VL 74 IS 24 BP 7669 EP 7674 DI 10.1128/AEM.01437-08 PG 6 WC Biotechnology & Applied Microbiology; Microbiology SC Biotechnology & Applied Microbiology; Microbiology GA 381CU UT WOS:000261513700027 PM 18836020 ER PT J AU Osipov, VV Muratov, CB AF Osipov, V. V. Muratov, C. B. TI Dynamic condensation blocking in cryogenic refueling SO APPLIED PHYSICS LETTERS LA English DT Article DE condensation; cryogenics; heat conduction ID EVAPORATION AB We demonstrate that a negative feedback between vapor pressure and condensation rate may be established in two-phase systems during vapor compression with rates of practical importance. As a result, dynamic condensation blocking occurs. The effect is studied numerically in the case of filling a no-vent insulated tank by liquid hydrogen. It is shown that the filling dynamics quite sensitively depends on the filling rate, and for sufficiently fast filling rates consist of a fast stage dominated by gas compression and a slow stage governed by heat conduction in the liquid. C1 [Osipov, V. V.] Mission Crit Technol Inc, El Segundo, CA 90245 USA. [Osipov, V. V.] NASA, Ames Res Ctr, Intelligent Syst Div, D&SH Branch, Moffett Field, CA 94035 USA. [Muratov, C. B.] New Jersey Inst Technol, Dept Math Sci, Newark, NJ 07102 USA. RP Osipov, VV (reprint author), Mission Crit Technol Inc, 2041 Rosecrans Ave,Suite 225, El Segundo, CA 90245 USA. EM muratov@njit.edu FU NSF [DMS-0718027] FX We are grateful to V.N. Smelyanskiy for suggesting this problem to us. The work of C. B. M. was supported, in part, by NSF via Grant No. DMS-0718027. NR 13 TC 3 Z9 3 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 0003-6951 J9 APPL PHYS LETT JI Appl. Phys. Lett. PD DEC 1 PY 2008 VL 93 IS 22 AR 224105 DI 10.1063/1.3025674 PG 3 WC Physics, Applied SC Physics GA 379XT UT WOS:000261430600095 ER PT J AU Mouroulis, P van Gorp, B Blaney, D Green, RO AF Mouroulis, Pantazis van Gorp, Byron Blaney, Diana Green, Robert O. TI Reflectance Microspectroscopy of Natural Rock Samples in the Visible and Near Infrared SO APPLIED SPECTROSCOPY LA English DT Article DE Reflectance spectroscopy; Microspectroscopy; Near-infrared region ID IMAGING SPECTROSCOPY; SURFACE AB We have collected reflectance spectra of various unprocessed rock samples in the 450-1650 nm wavelength range with a spatial resolution of 60 and 120 mu m (diameter) and using three illumination modes. Spectra taken in diffuse reflectance (dark field) mode are comparable to those obtained from macroscopic measurements and can provide the basis for mineral detection at that spatial scale. The spectral discrimination of the dark field mode is demonstrated to be consistent with the spatial resolution of the microscope for the samples examined. These results support the conclusion that reflectance microspectroscopy in the visible and near-infrared regions can be a valuable tool for understanding mineral formation at the spatial scale of tens of micrometers. C1 [Mouroulis, Pantazis; van Gorp, Byron; Blaney, Diana; Green, Robert O.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Mouroulis, P (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM zakos@jpl.nasa.gov FU National Aeronautics and Space Administration FX The research described here has been performed at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. NR 22 TC 4 Z9 4 U1 1 U2 7 PU SOC APPLIED SPECTROSCOPY PI FREDERICK PA 201B BROADWAY ST, FREDERICK, MD 21701 USA SN 0003-7028 J9 APPL SPECTROSC JI Appl. Spectrosc. PD DEC PY 2008 VL 62 IS 12 BP 1370 EP 1377 PG 8 WC Instruments & Instrumentation; Spectroscopy SC Instruments & Instrumentation; Spectroscopy GA 382GT UT WOS:000261594500013 PM 19094397 ER PT J AU Datiles, MB Ansari, RR Suh, KI Vitale, S Reed, GF Zigler, JS Ferris, FL AF Datiles, Manuel B., III Ansari, Rafat R. Suh, Kwang I. Vitale, Susan Reed, George F. Zigler, J. Samuel, Jr. Ferris, Frederick L., III TI Clinical Detection of Precataractous Lens Protein Changes Using Dynamic Light Scattering SO ARCHIVES OF OPHTHALMOLOGY LA English DT Article; Proceedings Paper CT Annual Meeting of the Association-for-Research-in-Vision-and-Ophthalmology CY MAY 06-10, 2007 CL Ft Lauderdale, FL SP Assoc Res Vis & Ophthalmol ID BOVINE ALPHA-CRYSTALLIN; AGE-RELATED-CHANGES; LIVING HUMAN LENS; MOLECULAR CHAPERONE; CATARACT FORMATION; GLUTATHIONE-REDUCTASE; NUCLEAR CATARACT; FUNCTIONAL-ROLE; OPACIFICATION; EYE AB Objective: To use dynamic light scattering to clinically assess early precataractous lens protein changes. Methods: We performed a cross-sectional study in 380 eyes of 235 patients aged 7 to 86 years with Age-Related Eye Disease Study clinical nuclear lens opacity grades 0 to 3.8. A dynamic light-scattering device was used to assess alpha-crystallin, a molecular chaperone protein shown to bind other damaged lens proteins, preventing their aggregation. The outcome measure was the alpha-crystallin index, a measure of unbound alpha-crystallin in each lens. The association of the alpha-crystallin index with increasing nuclear opacity and aging was determined. Results: There was a significant decrease in the alpha-crystallin index associated with increasing nuclear lens opacity grades (P<.001). There were significant losses of alpha-crystallin even in clinically clear lenses associated with aging (P<.001). The standard error of measurement was 3%. Conclusions: Dynamic light scattering clinically detects alpha-crystallin protein loss even in clinically clear lenses. alpha-Crystallin index measurements may be useful in identifying patients at high risk for cataracts and as an outcome variable in clinical lens studies. C1 [Datiles, Manuel B., III; Vitale, Susan; Reed, George F.; Zigler, J. Samuel, Jr.; Ferris, Frederick L., III] NEI, NIH, Bethesda, MD 20892 USA. [Ansari, Rafat R.] NASA, John H Glenn Res Ctr Lewis Field, Cleveland, OH USA. [Suh, Kwang I.] Ohio Aerosp Inst, Cleveland, OH USA. RP Datiles, MB (reprint author), NEI, NIH, 10 Ctr Dr,Bldg 10,Room 10N226, Bethesda, MD 20892 USA. EM DatilesM@NEI.NIH.GOV OI Datiles, Manuel III B./0000-0003-4660-1664 FU Intramural NIH HHS [Z99 EY999999] NR 52 TC 36 Z9 37 U1 1 U2 6 PU AMER MEDICAL ASSOC PI CHICAGO PA 515 N STATE ST, CHICAGO, IL 60610-0946 USA SN 0003-9950 J9 ARCH OPHTHALMOL-CHIC JI Arch. Ophthalmol. PD DEC PY 2008 VL 126 IS 12 BP 1687 EP 1693 DI 10.1001/archophthalmol.2008.507 PG 7 WC Ophthalmology SC Ophthalmology GA 380RA UT WOS:000261481700011 PM 19064850 ER PT J AU Hausrath, EM Treiman, AH Vicenzi, E Bish, DL Blake, D Sarrazin, P Hoehler, T Midtkandal, I Steele, A Brantley, SL AF Hausrath, E. M. Treiman, A. H. Vicenzi, E. Bish, D. L. Blake, D. Sarrazin, P. Hoehler, T. Midtkandal, I. Steele, A. Brantley, S. L. TI Short- and Long-Term Olivine Weathering in Svalbard: Implications for Mars SO ASTROBIOLOGY LA English DT Article DE Olivine; Weathering; Mars; Glass; Hydrothermal; CheMin ID FORSTERITE DISSOLUTION RATES; ARCTIC ALPINE ENVIRONMENT; AQUEOUS ALTERATION; NORTHERN SCANDINAVIA; SILICATE SURFACES; RIND DEVELOPMENT; SWEDISH LAPLAND; ORGANIC-ACIDS; GUSEV CRATER; PH AB Liquid water is essential to life as we know it on Earth; therefore, the search for water on Mars is a critical component of the search for life. Olivine, a mineral identified as present on Mars, has been proposed as an indicator of the duration and characteristics of water because it dissolves quickly, particularly under low-pH conditions. The duration of olivine persistence relative to glass under conditions of aqueous alteration reflects the pH and temperature of the reacting fluids. In this paper, we investigate the utility of 3 methodologies to detect silicate weathering in a Mars analog environment (Sverrefjell volcano, Svalbard). CheMin, a miniature Xray diffraction instrument developed for flight on NASA's upcoming Mars Science Laboratory, was deployed on Svalbard and was successful in detecting olivine and weathering products. The persistence of olivine and glass in Svalbard rocks was also investigated via laboratory observations of weathered hand samples as well as an in situ burial experiment. Observations of hand samples are consistent with the inference that olivine persists longer than glass at near-zero temperatures in the presence of solutions at pH similar to 7-9 on Svalbard, whereas in hydrothermally altered zones, glass has persisted longer than olivine in the presence of fluids at similar pH at similar to 50 degrees C. Analysis of the surfaces of olivine and glass samples, which were buried on Sverrefjell for 1 year and then retrieved, documented only minor incipient weathering, though these results suggest the importance of biological impacts. The 3 types of observations ( CheMin, laboratory observations of hand samples, burial experiments) of weathering of olivine and glass at Svalbard show promise for interpretation of weathering on Mars. Furthermore, the weathering relationships observed on Svalbard are consistent with laboratory-measured dissolution rates, which suggests that relative mineral dissolution rates in the laboratory, in concert with field observations, can be used to yield valuable information regarding the pH and temperature of reacting martian fluids. C1 [Hausrath, E. M.; Brantley, S. L.] Penn State Univ, Dept Geosci, University Pk, PA 16802 USA. [Hausrath, E. M.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. [Treiman, A. H.] Lunar & Planetary Inst, Houston, TX 77058 USA. [Vicenzi, E.] Smithsonian Inst, Natl Museum Nat Hist, Dept Mineral Sci, Washington, DC 20560 USA. [Bish, D. L.] Indiana Univ, Dept Geol Sci, Bloomington, IN 47405 USA. [Blake, D.; Hoehler, T.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Sarrazin, P.] InXitu Inc, Mountain View, CA USA. [Midtkandal, I.] Univ Oslo, Dept Geosci, Oslo, Norway. [Steele, A.] Carnegie Inst Washington, Geophys Lab, Washington, DC 20015 USA. RP Hausrath, EM (reprint author), Univ Nevada, Dept Geosci, 4505 S Maryland Pkwy, Las Vegas, NV 89154 USA. EM Elisabeth.Hausrath@unlv.edu FU World Universities Network, BRIE [DGE-9972759]; Pennsylvania State Astrobiology Research Center, NASA [NNG05GN72G]; NAI Research Fellowship; NSF Graduate Research Fellowship Program FX We would like to thank B. Abbey, M. Angelone, J. Cantolina, D. Voight, C. Lernhihan, A. Barnes, V. Bojan, T. Daniels, C. Winslow, V. Starke, and AMASE. We appreciate the thoughtful reviews by two anonymous reviewers and Hojatollah Vali. This work was supported by funding from the World Universities Network, BRIE [ Pennsylvania State NSF (IGERT) grant DGE-9972759], Pennsylvania State Astrobiology Research Center, NASA Grant NNG05GN72G, and the NAI Research Fellowship. E. M. H. is grateful for support from the NSF Graduate Research Fellowship Program. NR 77 TC 19 Z9 19 U1 3 U2 18 PU MARY ANN LIEBERT INC PI NEW ROCHELLE PA 140 HUGUENOT STREET, 3RD FL, NEW ROCHELLE, NY 10801 USA SN 1531-1074 J9 ASTROBIOLOGY JI Astrobiology PD DEC PY 2008 VL 8 IS 6 BP 1079 EP 1092 DI 10.1089/ast.2007.0195 PG 14 WC Astronomy & Astrophysics; Biology; Geosciences, Multidisciplinary SC Astronomy & Astrophysics; Life Sciences & Biomedicine - Other Topics; Geology GA 409OX UT WOS:000263516800003 PM 19191538 ER PT J AU Allen, CC Oehler, DZ AF Allen, Carlton C. Oehler, Dorothy Z. TI A Case for Ancient Springs in Arabia Terra, Mars SO ASTROBIOLOGY LA English DT Article DE Mars; Martian; Vernal Crater; Arabia Terra; Springs; Thermal springs; Warm springs; Spring mounds; HiRISE; Hot springs; Astrobiology ID HOT-SPRINGS; MERIDIANI PLANUM; THERMAL SPRINGS; IMPACT CRATER; DEPOSITS; LIFE; PRESERVATION; SEARCH; SILICIFICATION; MORPHOLOGIES AB Based on new image data from the High Resolution Imaging Science Experiment (HiRISE) on Mars Reconnaissance Orbiter (MRO), a case can be made that several structures in Vernal Crater, Arabia Terra are ancient springs. This interpretation is based on comprehensive geomorphologic analysis coupled with assessment of multiple hypotheses. The structures identified extend across several kilometers and are exceptional in that nothing with their detail and scale has been reported from Mars. The deposits are associated with an extensive fracture system that may have facilitated upward flow of warm fluids. Several additional spring-like features occur in Vernal Crater, and it is possible that these are part of a major province of spring activity. Since springs are environments where life could have evolved on Mars, where that life could have found refuge as the climate became colder and drier, and where signatures of that life may be preserved, Vernal Crater may be a site of major astrobiological importance. C1 [Allen, Carlton C.; Oehler, Dorothy Z.] NASA, Lyndon B Johnson Space Ctr, Astromat Res & Explorat Sci Directorate, Houston, TX 77058 USA. RP Allen, CC (reprint author), NASA, Lyndon B Johnson Space Ctr, Astromat Res & Explorat Sci Directorate, Houston, TX 77058 USA. EM carlton.c.allen@nasa.gov FU NASA; Astromaterials Research and Exploration Science Directorate; Johnson Space Center (JSC); NASA fellowship FX We thank NASA and the Astromaterials Research and Exploration Science Directorate at the Johnson Space Center (JSC) for support. We are grateful to Dr. Adrian Brown ( NASA Ames Research Center and SETI Institute) for assistance with CRISM interpretation, Dr. Mary Bourke ( Planetary Science Institute) and Ms. Jaclyn Allen ( JSC) for examining images of the spring-like features in Vernal Crater, Dr. Devon Burr for helpful comments and insights, and Mr. Orrin Thomas ( JSC Image Science and Analysis Group) for 3-D analysis of CTX images. The manuscript was reviewed by Dr. Stephen Grasby ( Geological Survey of Canada), Dr. Larry Crumpler ( New Mexico Museum of Natural History and Science), and an anonymous reviewer, all of whom made important comments and suggestions. We are grateful to Dr. David Beaty (NASA-JPL) for helpful discussions, Dr. M. A. (Rien) Habermehl ( Australian Government Department of Agriculture, Fisheries and Forestry) for providing information about springs in the Great Artesian Basin and at Dalhousie, and Dr. Malcolm Walter ( Australian Centre for Astrobiology) for encouragement. We thank Google Earth for permission to use some of their images. This work was partially funded by a NASA fellowship to D. Z. O. NR 83 TC 39 Z9 40 U1 2 U2 10 PU MARY ANN LIEBERT, INC PI NEW ROCHELLE PA 140 HUGUENOT STREET, 3RD FL, NEW ROCHELLE, NY 10801 USA SN 1531-1074 EI 1557-8070 J9 ASTROBIOLOGY JI Astrobiology PD DEC PY 2008 VL 8 IS 6 BP 1093 EP 1112 DI 10.1089/ast.2008.0239 PG 20 WC Astronomy & Astrophysics; Biology; Geosciences, Multidisciplinary SC Astronomy & Astrophysics; Life Sciences & Biomedicine - Other Topics; Geology GA 409OX UT WOS:000263516800004 PM 19093802 ER PT J AU Kempf, MJ Schubert, WW Beaudet, RA AF Kempf, M. J. Schubert, W. W. Beaudet, R. A. TI Determination of Lethality Rate Constants and D-Values for Bacillus atrophaeus (ATCC 9372) Spores Exposed to Dry Heat from 115 degrees C to 170 degrees C SO ASTROBIOLOGY LA English DT Article DE Bacillus atrophaeus spores; Planetary protection; Dry heat microbial reduction ID SUBTILIS VAR NIGER; AIRBORNE BACTERIAL-SPORES; THERMAL-RESISTANCE; WATER ACTIVITIES; INACTIVATION; KINETICS; MICROORGANISMS; STERILIZATION; REQUIREMENTS; HUMIDITY AB Dry heat microbial reduction is the NASA-approved sterilization method to reduce the microbial bioburden on spaceflight hardware for missions with planetary protection requirements. The method involves heating the spaceflight hardware to temperatures between 104 degrees C and 125 degrees C for up to 50 hours, while controlling the humidity to very low values. Collection of lethality data at temperatures above 125 degrees C and with ambient ( uncontrolled) humidity conditions would establish whether any microbial reduction credit can be offered to the flight project for processes that occur at temperatures greater than 125 degrees C. The goal of this research is to determine the survival rates of Bacillus atrophaeus ( ATCC 9372) spores subjected to temperatures higher than 125 degrees C under both dry (controlled) and room ambient humidity (36-66% relative humidity) conditions. Spores were deposited inside thin, stainless steel thermal spore exposure vessels (TSEVs) and heated under ambient or controlled humidity conditions from 115 degrees C to 170 degrees C. After the exposures, the TSEVs were cooled rapidly, and the spores were recovered and plated. Survivor ratios, lethality rate constants, and D-values were calculated at each temperature. At 115 degrees C and 125 degrees C, the controlled humidity lethality rate constant was faster than the ambient humidity lethality rate constant. At 135 degrees C, the ambient and controlled humidity lethality rate constants were statistically identical. At 150 degrees C and 170 degrees C, the ambient humidity lethality rate constant was slightly faster than the controlled humidity lethality rate constant. These results provide evidence for possibly modifying the NASA dry heat microbial reduction specification. C1 [Kempf, M. J.; Schubert, W. W.; Beaudet, R. A.] CALTECH, Jet Prop Lab, Biotechnol & Planetary Protect Grp, Pasadena, CA USA. RP Kempf, MJ (reprint author), Univ Tennessee, Dept Biol Sci, 574 Univ St,228 Brehm Hall, Martin, TN 38238 USA. EM mkempf@utm.edu NR 37 TC 11 Z9 11 U1 1 U2 10 PU MARY ANN LIEBERT INC PI NEW ROCHELLE PA 140 HUGUENOT STREET, 3RD FL, NEW ROCHELLE, NY 10801 USA SN 1531-1074 J9 ASTROBIOLOGY JI Astrobiology PD DEC PY 2008 VL 8 IS 6 BP 1169 EP 1182 DI 10.1089/ast.2007.0208 PG 14 WC Astronomy & Astrophysics; Biology; Geosciences, Multidisciplinary SC Astronomy & Astrophysics; Life Sciences & Biomedicine - Other Topics; Geology GA 409OX UT WOS:000263516800009 PM 19191542 ER PT J AU Mengel, S Lehnert, MD Thatte, N Whitmore, B Vacca, WD Chandar, R AF Mengel, S. Lehnert, M. D. Thatte, N. Whitmore, B. Vacca, W. D. Chandar, R. TI Young star clusters in the Antennae galaxies and NGC 1487 SO ASTRONOMISCHE NACHRICHTEN LA English DT Article DE galaxies: individual (Antennae, NGC 1487); galaxies: kinematics and dynamics; galaxies: star clusters ID STELLAR CLUSTERS; MASS-LOSS; NGC-4038/4039; M82; SPECTROSCOPY; DESTRUCTION; STARBURST; IMPACT; SIZES AB We estimate the dynamical masses of several young (approximate to 10 Myr) massive star clusters in two interacting galaxies, NGC 4038/4039 ("The Antennae") and NGC 1487, under the assumption of virial equilibrium. These are compared with photometric mass estimates. A dynamical mass substantially higher than the photometric estimate could indicate non-virial motion of the stars in the cluster, and potentially lead to cluster disruption. All but one of the Antennae clusters have dynamical and photometric mass estimates which are within a factor approximate to 2 of one another, implying both that standard IMFs provide a good approximation to the IMF of these clusters, and that there is no significant extra-virial motion, as would be expected if they were rapidly dispersing. These results suggest that almost all of the clusters in our sample have survived the gas removal phase as bound or marginally bound objects. But a few targets (two in NGC 1487 and one in the Antennae) have M(dyn) estimates which are significantly larger than the photometric mass estimates. At least two of those clusters may be actively in the process of dissolving. The dissolution candidates in both galaxies are amongst the clusters with the lowest pressures/densities measured in our sample. (C) 2008 WILEY-VCH Verlag GmbH & Co. KGaA, Weinheim C1 [Mengel, S.] European So Observ, D-85748 Garching, Germany. [Lehnert, M. D.] Univ Paris 07, CNRS, Observ Paris, F-92190 Meudon, France. [Thatte, N.] Univ Oxford, Dept Astrophys, Gb Oxford OX1 3RH, England. [Whitmore, B.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Vacca, W. D.] Univ Space Res Assoc, NASA, Ames Res Ctr, Stratospher Observ Infrared Astron, Moffett Field, CA 94035 USA. [Chandar, R.] Univ Toledo, Toledo, OH 43606 USA. RP Mengel, S (reprint author), European So Observ, Karl Schwarzschild Str 2, D-85748 Garching, Germany. EM smengel@eso.org NR 25 TC 0 Z9 0 U1 0 U2 1 PU WILEY-V C H VERLAG GMBH PI WEINHEIM PA PO BOX 10 11 61, D-69451 WEINHEIM, GERMANY SN 0004-6337 J9 ASTRON NACHR JI Astro. Nachr. PD DEC PY 2008 VL 329 IS 9-10 BP 944 EP 947 DI 10.1002/asna.200811072 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 399IY UT WOS:000262794800017 ER PT J AU Krucker, S Battaglia, M Cargill, PJ Fletcher, L Hudson, HS MacKinnon, AL Masuda, S Sui, L Tomczak, M Veronig, AL Vlahos, L White, SM AF Krucker, S. Battaglia, M. Cargill, P. J. Fletcher, L. Hudson, H. S. MacKinnon, A. L. Masuda, S. Sui, L. Tomczak, M. Veronig, A. L. Vlahos, L. White, S. M. TI Hard X-ray emission from the solar corona SO ASTRONOMY AND ASTROPHYSICS REVIEW LA English DT Review DE Sun; Corona; Hard X-rays ID HIGH-ENERGY ELECTRONS; COLLAPSING MAGNETIC TRAPS; FAST-MODE WAVES; LOOP-TOP SOURCE; 2002 JULY 23; PARTICLE-ACCELERATION; IMPULSIVE PHASE; SPECTRAL EVOLUTION; STOCHASTIC ACCELERATION; CURRENT SHEETS AB This review surveys hard X-ray emissions of non-thermal electrons in the solar corona. These electrons originate in flares and flare-related processes. Hard X-ray emission is the most direct diagnostic of electron presence in the corona, and such observations provide quantitative determinations of the total energy in the non-thermal electrons. The most intense flare emissions are generally observed from the chromosphere at footpoints of magnetic loops. Over the years, however, many observations of hard X-ray and even gamma-ray emission directly from the corona have also been reported. These coronal sources are of particular interest as they occur closest to where the electron acceleration is thought to occur. Prior to the actual direct imaging observations, disk occultation was usually required to study coronal sources, resulting in limited physical information. Now RHESSI has given us a systematic view of coronal sources that combines high spatial and spectral resolution with broad energy coverage and high sensitivity. Despite the low density and hence low bremsstrahlung efficiency of the corona, we now detect coronal hard X-ray emissions from sources in all phases of solar flares. Because the physical conditions in such sources may differ substantially from those of the usual "footpoint" emission regions, we take the opportunity to revisit the physics of hard X-radiation and relevant theories of particle acceleration. C1 [Krucker, S.; Hudson, H. S.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Battaglia, M.] Swiss Fed Inst Technol, Inst Astron, CH-8093 Zurich, Switzerland. [Cargill, P. J.] Univ London Imperial Coll Sci Technol & Med, Blackett Lab, London SW7 2BW, England. [MacKinnon, A. L.] Univ Glasgow, Dept Phys & Astron, DACE, Glasgow G12 8QQ, Lanark, Scotland. [Masuda, S.] Nagoya Univ, Solar Terr Environm Lab, Chikusa Ku, Nagoya, Aichi 4648601, Japan. [Sui, L.] NASA, Goddard Space Flight Ctr, Solar Phys Lab, Greenbelt, MD 20771 USA. [Tomczak, M.] Univ Wroclaw, Astron Inst, PL-51622 Wroclaw, Poland. [Veronig, A. L.] Graz Univ, Inst Phys, IGAM, A-8010 Graz, Austria. [Vlahos, L.] Univ Thessaloniki, Dept Phys, Thessaloniki 54124, Greece. [White, S. M.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. RP Krucker, S (reprint author), Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. EM krucker@ssl.berkeley.edu RI Veronig, Astrid/B-8422-2009; OI Battaglia, Marina/0000-0003-1438-9099 NR 221 TC 110 Z9 110 U1 1 U2 6 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0935-4956 EI 1432-0754 J9 ASTRON ASTROPHYS REV JI Astron. Astrophys. Rev. PD DEC PY 2008 VL 16 IS 3-4 BP 155 EP 208 DI 10.1007/s00159-008-0014-9 PG 54 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 379WL UT WOS:000261426800001 ER PT J AU Beckmann, V Courvoisier, TJL Gehrels, N Lubinski, P Malzac, J Petrucci, PO Shrader, CR Soldi, S AF Beckmann, V. Courvoisier, T. J. -L. Gehrels, N. Lubinski, P. Malzac, J. Petrucci, P. -O. Shrader, C. R. Soldi, S. TI The efficient low-mass Seyfert MCG-05-23-016 SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE galaxies: active; galaxies: Seyfert; X-rays: galaxies; galaxies: individual: MCG-05-23-016; accretion, accretion discs ID ACTIVE GALACTIC NUCLEI; X-RAY SOURCES; BLACK-HOLE MASS; BEPPOSAX OBSERVATIONS; INTEGRAL OBSERVATIONS; VELOCITY DISPERSION; GALAXY MCG-5-23-16; COMPTON REFLECTION; EMISSION; SPECTRA AB Aims. The Seyfert 1.9 galaxy MCG-05-23-016 has been shown to exhibit a complex X-ray spectrum. This source has moderate X-ray luminosity, hosts a comparably low-mass black hole, but accretes at a high Eddington rate, and allows us to study a super massive black hole in an early stage. Methods. Three observations of the INTEGRAL satellite simultaneous with pointed Swift/XRT observations performed from December 2006 to June 2007 are used in combination with public data from the INTEGRAL archive to study the variability of the hard X-ray components and to generate a high-quality spectrum from 1 to 150 keV. Results. The AGN shows little variability in the hard X-ray spectrum, with some indication of a variation in the high-energy cut-of energy ranging from 50 keV to >> 100 keV, with an electron plasma temperature in the 10-90 keV range. The reflection component is not evident and, if present, the reflected fraction can be constrained to R < 0.3 for the combined data set. Comparison to previous observations shows that the reflection component has to be variable. No variability in the UV and optical range is observed on a time scale of 1.5 years. Conclusions. The hard X-ray spectrum of MCG-05-23-016 appears to be stable with the luminosity and underlying power law varying moderately and the optical/UV flux staying constant. The reflection component and the iron K alpha line seem to have decreased between December 2005 and the observations presented here. The spectral energy distribution appears to be similar to that of Galactic black hole systems, e. g. XTE 1118+ 480 in the low state. The AGN exhibits a remarkably high Eddington ratio of L-bol/L-Edd greater than or similar to 0.8 (or L-bol/L-Edd greater than or similar to 0.1, if we consider a higher mass of the central engine) and, at the same time, a low cut-off energy around 70 keV. Objects like MCG-05-23-016 might indicate the early stages of super massive black holes, in which a strong accretion flow feeds the central engine. C1 [Beckmann, V.; Courvoisier, T. J. -L.; Lubinski, P.; Soldi, S.] ISDC Data Ctr Astrophys, CH-1290 Versoix, Switzerland. [Beckmann, V.; Courvoisier, T. J. -L.; Soldi, S.] Univ Geneva, Astron Observ, CH-1290 Sauverny, Switzerland. [Beckmann, V.] Univ Maryland Baltimore Cty, Baltimore, MD 21250 USA. [Gehrels, N.; Shrader, C. R.] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA. [Lubinski, P.] Ctr Astron M Kopernika, PL-00716 Warsaw, Poland. [Malzac, J.] CNRS, UPS, OMP, Ctr Etud Spatiale Rayonnements, F-31028 Toulouse 4, France. [Petrucci, P. -O.] Univ Grenoble 1, CNRS, UMR 5571, Lab Astrophys Grenoble, F-38041 Grenoble, France. RP Beckmann, V (reprint author), ISDC Data Ctr Astrophys, Chemin Ecogia 16, CH-1290 Versoix, Switzerland. EM Volker.Beckmann@unige.ch RI Gehrels, Neil/D-2971-2012 NR 52 TC 8 Z9 8 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 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD DEC PY 2008 VL 492 IS 1 BP 93 EP 99 DI 10.1051/0004-6361:200810674 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 377LQ UT WOS:000261253100015 ER PT J AU Kreykenbohm, I Wilms, J Kretschmar, P Torrejon, JM Pottschmidt, K Hanke, M Santangelo, A Ferrigno, C Staubert, R AF Kreykenbohm, I. Wilms, J. Kretschmar, P. Torrejon, J. M. Pottschmidt, K. Hanke, M. Santangelo, A. Ferrigno, C. Staubert, R. TI High variability in Vela X-1: giant flares and off states SO ASTRONOMY & ASTROPHYSICS LA English DT Review DE X-rays: stars; stars: flare; stars: pulsars: individual: Vela X-1; stars: magnetic fields ID X-RAY PULSARS; QUASI-PERIODIC OSCILLATIONS; CYCLOTRON-LINE FEATURES; CLUMPY STELLAR WINDS; INTEGRAL OBSERVATION; NEUTRON-STAR; CIRCUMSTELLAR MATTER; MAGNETIC-FIELDS; OUTER EVOLUTION; ACCRETION FLOW AB Aims. We investigate the spectral and temporal behavior of the high mass X-ray binary Vela X-1 during a phase of high activity, with special focus on the observed giant flares and off states. Methods. INTEGRAL observed Vela X-1 in a long almost uninterrupted observation for two weeks in 2003 Nov/Dec. The data were analyzed with OSA 7.0 and FTOOLS 6.2. We derive the pulse period, light curves, spectra, hardness ratios, and hardness intensity diagrams, and study the eclipse. Results. In addition to an already high activity level, Vela X-1 exhibited several intense flares, the brightest ones reaching a maximum intensity of more than 5 Crab in the 20-40 keV band and several off states where the source was no longer detected by INTEGRAL. We determine the pulse period to be 283.5320 +/- 0.0002 s, which is stable throughout the entire observation. Analyzing the eclipses provided an improvement in the ephemeris. Spectral analysis of the flares indicates that there appear to be two types of flares: relatively brief flares, which can be extremely intense and show spectral softening, in contrast to high intensity states, which are longer and show no softening. Conclusions. Both flares and off states are interpreted as being due to a strongly structured wind of the optical companion. When Vela X-1 encounters a cavity with strongly reduced density, the flux will drop triggering the onset of the propeller effect, which inhibits further accretion, giving rise to off states. The sudden decrease in the density of the material required to trigger the propeller effect in Vela X-1 is of the same order as predicted by theoretical papers about the densities in OB star winds. A similarly structured wind can produce giant flares when Vela X-1 encounters a dense blob in the wind. C1 [Kreykenbohm, I.; Wilms, J.; Hanke, M.] Dr Karl Remeis Sternwarte Bamberg, D-96049 Bamberg, Germany. [Kreykenbohm, I.; Wilms, J.; Hanke, M.] Erlangen Ctr Astroparticle Phys, D-91058 Erlangen, Germany. [Kreykenbohm, I.; Santangelo, A.; Ferrigno, C.; Staubert, R.] Inst Astron & Astrophys, Kepler Ctr Astro & Particle Phys, D-72076 Tubingen, Germany. [Kreykenbohm, I.; Ferrigno, C.] INTEGRAL Sci Data Ctr, CH-1290 Chavannes Des Bois, Switzerland. [Kretschmar, P.] European Space Astron Ctr, European Space Agcy, Madrid 28691, Spain. [Torrejon, J. M.] Univ Alicante, Escuela Politecn Super, Dept Fis Ingn Sistemas & Teoria Senal, Alicante 03080, Spain. [Torrejon, J. M.] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. [Pottschmidt, K.] Univ Maryland, CRESST, Baltimore, MD 21250 USA. [Pottschmidt, K.] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA. [Ferrigno, C.] IASF INAF, I-90136 Palermo, Italy. RP Kreykenbohm, I (reprint author), Dr Karl Remeis Sternwarte Bamberg, Sternwartstr 7, D-96049 Bamberg, Germany. EM Ingo.Kreykenbohm@sternwarte.uni-erlangen.de RI Ferrigno, Carlo/H-4139-2012; Wilms, Joern/C-8116-2013; Kreykenbohm, Ingo/H-9659-2013; Torrejon, Jose /K-6395-2014; OI Wilms, Joern/0000-0003-2065-5410; Kreykenbohm, Ingo/0000-0001-7335-1803; Torrejon, Jose /0000-0002-5967-5163; Kretschmar, Peter/0000-0001-9840-2048 NR 115 TC 63 Z9 63 U1 0 U2 1 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD DEC PY 2008 VL 492 IS 2 BP 511 EP 525 DI 10.1051/0004-6361:200809956 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 379YC UT WOS:000261431500023 ER PT J AU Piranomonte, S Ward, PA Fiore, F Vergani, SD D'Elia, V Krongold, Y Nicastro, F Meurs, EJA Chincarini, G Covino, S Della Valle, M Fugazza, D Norci, L Sbordone, L Stella, L Tagliaferri, G Burrows, DN Gehrels, N Goldoni, P Malesani, D Mirabel, IF Pellizza, LJ Perna, R AF Piranomonte, S. Ward, P. A. Fiore, F. Vergani, S. D. D'Elia, V. Krongold, Y. Nicastro, F. Meurs, E. J. A. Chincarini, G. Covino, S. Della Valle, M. Fugazza, D. Norci, L. Sbordone, L. Stella, L. Tagliaferri, G. Burrows, D. N. Gehrels, N. Goldoni, P. Malesani, D. Mirabel, I. F. Pellizza, L. J. Perna, R. TI Probing the complex environments of GRB host galaxies and intervening systems: high resolution spectroscopy of GRB050922C SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE gamma rays: bursts; cosmology: observations; galaxies: abundances; galaxies: ISM ID GAMMA-RAY BURSTS; PHOTOCHEMICAL EVOLUTION; PHYSICAL CONDITIONS; LEVEL POPULATIONS; ELLIPTIC GALAXIES; AFTERGLOW; GRB-021004; PROGENITOR; REDSHIFT; PHOTOIONIZATION AB Aims. The aim of this paper is to investigate the environment of gamma ray bursts (GRBs) and the interstellar matter of their host galaxies. Methods. To this purpose we use high resolution spectroscopic observations of the afterglow of GRB050922C, obtained with UVES/VLT similar to 3.5 h after the GRB event. Results. We found that, as for most high resolution spectra of GRBs, the spectrum of the afterglow of GRB050922C is complex. At least seven components contribute to the main absorption system at z = 2.1992. The detection of lines of neutral elements like MgI and the detection of fine-structure levels of the ions FeII, SiII and CII allows us to separate components in the GRB ISM along the line of sight. Moreover, in addition to the main system, we analyzed the five intervening systems between z = 2.077 and z = 1.5664 identified along the GRB line of sight. Conclusions. GRB afterglow spectra are very complex, but full of information. This can be used to disentangle the contribution of the different parts of the GRB host galaxy and to study their properties. Our metallicity estimates agree with the scenario of GRBs exploding in low metallicity galaxies C1 [Piranomonte, S.; Fiore, F.; D'Elia, V.; Nicastro, F.; Stella, L.] Osserv Astron Roma, INAF, I-00040 Monte Porzio Catone, RM, Italy. [Ward, P. A.] Univ Coll London, Mullard Space Sci Lab, Dorking RH5 6NT, Surrey, England. [Vergani, S. D.; Norci, L.] Dublin Inst Adv Studies, Dublin 2, Ireland. [Vergani, S. D.; Meurs, E. J. A.] Dublin City Univ, Sch Phys Sci, Dublin 9, Ireland. [Vergani, S. D.; Meurs, E. J. A.] Dublin City Univ, NCPST, Dublin 9, Ireland. [Vergani, S. D.; Chincarini, G.; Covino, S.; Fugazza, D.; Tagliaferri, G.] Osserv Astron Brera, INAF, I-23807 Merate, LC, Italy. [Krongold, Y.] Univ Nacl Autonoma Mexico, Astron Inst, Mexico City 04510, DF, Mexico. [Chincarini, G.] Univ Milan, I-20126 Milan, Italy. [Della Valle, M.] Osserv Astron Capodimonte, INAF, I-80131 Naples, Italy. [Della Valle, M.] Int Ctr Relativist Astrophys Network, I-65122 Pescara, Italy. [Della Valle, M.] European So Observ, D-85748 Garching, Germany. [Sbordone, L.] Univ Paris Diderot, CNRS, Observ Paris, GEPI, F-92190 Meudon, France. [Burrows, D. N.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Gehrels, N.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Goldoni, P.] Lab Astroparticule & Cosmol, UMR 7164, APC, F-75231 Paris 05, France. [Goldoni, P.] CEA Saclay, DSM, DAPNIA, Serv Astrophys, F-91191 Gif Sur Yvette, France. [Malesani, D.] Niels Bohr Inst, Dark Cosmol Ctr, DK-2100 Copenhagen O, Denmark. [Mirabel, I. F.] European So Observ, Santiago 19, Chile. [Pellizza, L. J.] Inst Astron & Fis Espacio, CONICET, UBA, RA-1428 Buenos Aires, DF, Argentina. [Perna, R.] Univ Colorado, JILA, Boulder, CO 80309 USA. RP Piranomonte, S (reprint author), Osserv Astron Roma, INAF, I-00040 Monte Porzio Catone, RM, Italy. EM piranomonte@oa-roma.inaf.it RI Gehrels, Neil/D-2971-2012; OI Nicastro, Fabrizio/0000-0002-6896-1364; D'Elia, Valerio/0000-0002-7320-5862; Della Valle, Massimo/0000-0003-3142-5020; Fiore, Fabrizio/0000-0002-4031-4157 FU MIUR [COFIN-03-02-23, INAF/PRIN270/2003]; ASI [ASI/I/R/039/04, ASI/I/R/023/05/0]; SFI FX We thank an anonymous referee for comments that improved the presentation. We thank C. Porciani, V. D'Odorico, H.-W. Chen, J. X. Prochaska and P. M. Vreeswijk for useful discussions. Part of this work was supported by MIUR COFIN-03-02-23 and INAF/PRIN270/2003 and ASI contracts ASI/I/R/039/04 and ASI/I/R/023/05/0. S. P. and V. D. acknowledge support from ASI grants. S. P., S. D. V. and M. D. V. thank the Dark Cosmology Centre of Copenhagen, where part of this work was done, for the friendly and creative atmosphere. D. M. acknowledges the Instrument Center for Danish Astrophysics for support and thanks the Dark Cosmology Centre (funded by the DNRF). S. D. V. is supported by SFI. NR 43 TC 28 Z9 28 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 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD DEC PY 2008 VL 492 IS 3 BP 775 EP 785 DI 10.1051/0004-6361:20079015 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 383UA UT WOS:000261697900020 ER PT J AU Goad, MR Tyler, LG Beardmore, AP Evans, PA Rosen, SR Osborne, JP Starling, RLC Marshall, FE Yershov, V Burrows, DN Gehrels, N Roming, PWA Moretti, A Capalbi, M Hill, JE Kennea, J Koch, S Berk, DV AF Goad, M. R. Tyler, L. G. Beardmore, A. P. Evans, P. A. Rosen, S. R. Osborne, J. P. Starling, R. L. C. Marshall, F. E. Yershov, V. Burrows, D. N. Gehrels, N. Roming, P. W. A. Moretti, A. Capalbi, M. Hill, J. E. Kennea, J. Koch, S. Berk, D. Vanden TI Accurate early positions for Swift GRBs: enhancing X-ray positions with UVOT astrometry (vol 476, pg 1401, 2007) SO ASTRONOMY & ASTROPHYSICS LA English DT Correction DE gamma rays: bursts; astrometry; errata, addenda C1 [Goad, M. R.; Tyler, L. G.; Beardmore, A. P.; Evans, P. A.; Rosen, S. R.; Osborne, J. P.; Starling, R. L. C.] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England. [Marshall, F. E.; Gehrels, N.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Rosen, S. R.; Yershov, V.] Univ Coll London, Mullard Space Sci Lab, Dept Space & Climate Phys, Dorking RH5 6NT, Surrey, England. [Burrows, D. N.; Roming, P. W. A.; Kennea, J.; Koch, S.; Berk, D. Vanden] Penn State Univ, University Pk, PA 16802 USA. [Moretti, A.] INAF Osservatorio Astronom Brera, I-23807 Merate, Lc, Italy. [Capalbi, M.] ASI Sci Data Ctr, I-00044 Frascati, Italy. [Hill, J. E.] Univ Space Res Assoc, Columbia, MD 21044 USA. RP Goad, MR (reprint author), Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England. EM mrg@star.le.ac.uk RI Gehrels, Neil/D-2971-2012 NR 1 TC 2 Z9 2 U1 0 U2 1 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD DEC PY 2008 VL 492 IS 3 BP 873 EP 873 DI 10.1051/0004-6361:20078436e PG 1 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 383UA UT WOS:000261697900029 ER PT J AU Smith, DA Guillemot, L Camilo, F Cognard, I Dumora, D Espinoza, C Freire, PCC Gotthelf, EV Harding, AK Hobbs, GB Johnston, S Kaspi, VM Kramer, M Livingstone, MA Lyne, AG Manchester, RN Marshall, FE McLaughlin, MA Noutsos, A Ransom, SM Roberts, MSE Romani, RW Stappers, BW Theureau, G Thompson, DJ Thorsett, SE Wang, N Weltevrede, P AF Smith, D. A. Guillemot, L. Camilo, F. Cognard, I. Dumora, D. Espinoza, C. Freire, P. C. C. Gotthelf, E. V. Harding, A. K. Hobbs, G. B. Johnston, S. Kaspi, V. M. Kramer, M. Livingstone, M. A. Lyne, A. G. Manchester, R. N. Marshall, F. E. McLaughlin, M. A. Noutsos, A. Ransom, S. M. Roberts, M. S. E. Romani, R. W. Stappers, B. W. Theureau, G. Thompson, D. J. Thorsett, S. E. Wang, N. Weltevrede, P. TI Pulsar timing for the Fermi gamma-ray space telescope SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE space vehicles: instruments; stars: pulsars: general; gamma-rays: observations; ephemerides ID RAPIDLY SPINNING PULSARS; GIANT RADIO PULSES; MILLISECOND PULSARS; HIGH-ENERGY; BINARY PULSAR; CRAB PULSAR; PRECISION; RADIATION; MODEL; DISCOVERY AB We describe a comprehensive pulsar monitoring campaign for the Large Area Telescope (LAT) on the Fermi Gamma-ray Space Telescope ( formerly GLAST). The detection and study of pulsars in gamma rays give insights into the populations of neutron stars and supernova rates in the Galaxy, into particle acceleration mechanisms in neutron star magnetospheres, and into the "engines" driving pulsar wind nebulae. LAT's unprecedented sensitivity between 20 MeV and 300 GeV together with its 2.4 sr field-of-view makes detection of many gamma-ray pulsars likely, justifying the monitoring of over two hundred pulsars with large spin-down powers. To search for gamma-ray pulsations from most of these pulsars requires a set of phase-connected timing solutions spanning a year or more to properly align the sparse photon arrival times. We describe the choice of pulsars and the instruments involved in the campaign. Attention is paid to verifications of the LAT pulsar software, using for example giant radio pulses from the Crab and from PSR B1937+21 recorded at Nancay, and using X-ray data on PSR J0218+4232 from XMM-Newton. We demonstrate accuracy of the pulsar phase calculations at the microsecond level. C1 [Smith, D. A.; Guillemot, L.; Dumora, D.] Univ Bordeaux, Ctr Etud Nucl Bordeaux Gradignan, UMR 5797, F-33175 Gradignan, France. [Smith, D. A.; Guillemot, L.; Dumora, D.] Ctr Etud Nucl Bordeaux Gradignan, IN2P3, CNRS, UMR 5797, F-33175 Gradignan, France. [Camilo, F.; Gotthelf, E. V.] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA. [Cognard, I.; Theureau, G.] CNRS INSU, UMR 6115, LPCE, F-45071 Orleans, France. [Cognard, I.; Theureau, G.] CNRS INSU, Observ Paris, Stn Radioastron Nancay, F-18330 Nancay, France. [Theureau, G.] Univ Paris Diderot, CNRS, Observ Paris, GEPI, F-92190 Meudon, France. [Espinoza, C.; Kramer, M.; Lyne, A. G.; Noutsos, A.; Stappers, B. W.] Univ Manchester, Jodrell Bank Observ, Macclesfield SK11 9DL, Cheshire, England. [Freire, P. C. C.] Arecibo Observ, Arecibo, PR 00612 USA. [Harding, A. K.; Marshall, F. E.; Thompson, D. J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Hobbs, G. B.; Johnston, S.; Manchester, R. N.; Weltevrede, P.] CSIRO, Australia Telescope Natl Facil, Epping, NSW 1710, Australia. [Kaspi, V. M.; Livingstone, M. A.] McGill Univ, Montreal, PQ, Canada. [McLaughlin, M. A.] W Virginia Univ, Dept Phys, Morgantown, WV 26506 USA. [Ransom, S. M.] Natl Radio Astron Observ, Charlottesville, VA 22903 USA. [Roberts, M. S. E.] Eureka Sci Inc, Oakland, CA 94602 USA. [Romani, R. W.] Stanford Univ, Dept Phys, Stanford, CA 94305 USA. [Thorsett, S. E.] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA. [Wang, N.] Chinese Acad Sci, Natl Astron Observ, Urumqi 830011, Peoples R China. RP Smith, DA (reprint author), Univ Bordeaux, Ctr Etud Nucl Bordeaux Gradignan, UMR 5797, F-33175 Gradignan, France. EM smith@cenbg.in2p3.fr RI Thompson, David/D-2939-2012; Harding, Alice/D-3160-2012; OI Thompson, David/0000-0001-5217-9135; Thorsett, Stephen/0000-0002-2025-9613; Roberts, Mallory/0000-0002-9396-9720; Ransom, Scott/0000-0001-5799-9714 NR 80 TC 77 Z9 78 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 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD DEC PY 2008 VL 492 IS 3 BP 923 EP 931 DI 10.1051/0004-6361:200810285 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 383UA UT WOS:000261697900032 ER PT J AU Hartman, RC Kadler, M Tueller, J AF Hartman, R. C. Kadler, M. Tueller, J. TI GAMMA-RAY EMISSION FROM THE BROAD-LINE RADIO GALAXY 3C 111 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: active; galaxies: individual (3C 111); gamma rays: observations ID SEYFERT-GALAXIES; SKY SURVEY; M87 JET; MISSION; TELESCOPE; CATALOG; 3C-111; CLOUD AB The broad-line radio galaxy 3C 111 has been suggested as the counterpart of the gamma-ray source 3EG J0416+3650. While 3C 111 meets most of the criteria for a high-probability identification, like a bright flat-spectrum radio core and a blazar-like broadband SED, in the Third EGRET Catalog, the large positional offset of about 1.5 degrees put 3C 111 outside the 99% probability region for 3EG J0416+3650, making this association questionable. We present a reanalysis of all available data for 3C 111 from the EGRET archives, resulting in probable detection of high-energy gamma-ray emission above 1000 MeV from a position close to the nominal position of 3C 111, in two separate viewing periods (VPs), at a 3 sigma level in each. A new source, GRO J0426+3747, appears to be present nearby, seen only in the >1000 MeV data. For >100 MeV, the data are in agreement with only one source ( at the original catalog position) accounting for most of the EGRET-detected emission of 3EG J0416+3650. A follow-up Swift UVOT/XRT observation reveals one moderately bright X-ray source in the error box of 3EG J0416+3650, but because of the large EGRET position uncertainty, it is not certain that the X-ray and gamma-ray sources are associated. A Swift observation of GRO J0426+3747 detected no X-ray source nearby. C1 [Hartman, R. C.; Tueller, J.] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA. [Kadler, M.] Univ Erlangen Nurnberg, Dr Karl Remeis Observ, D-96049 Bamberg, Germany. [Kadler, M.] NASA, Goddard Space Flight Ctr, CRESST, Greenbelt, MD 20771 USA. [Kadler, M.] Univ Space Res Assoc, Columbia, MD 21044 USA. RP Hartman, RC (reprint author), NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Code 661, Greenbelt, MD 20771 USA. RI Tueller, Jack/D-5334-2012; OI Kadler, Matthias/0000-0001-5606-6154 FU NASA Postdoctoral Program at the Goddard Space Flight Center; NSF; Smithsonian Institution; Academia Sinica FX We thank Goro Sato, Francesco Verrecchia, Svetlana Jorstad, and Chris Shrader for their help and advice in compiling the SED data for this study. Steve Drake and Rachel Osten have kindly provided insight regarding X-ray emission from stars. M. K. has been supported by the NASA Postdoctoral Program at the Goddard Space Flight Center, administered by Oak Ridge Associated Universities through a contract with NASA. This research has made use of data obtained from the High Energy Astrophysics Science Archive Research Center (HEASARC), provided by the NASA Goddard Space Flight Center, and the NASA/IPAC Extragalactic Database (NED), operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with NASA. We have also made use of data products from the Two Micron All Sky Survey, a joint project of the University of Massachusetts and the Infrared Processing and Analysis Center, California Institute of Technology, funded by NASA and NSF. Submillimeter flux ranges for 3C 111 were obtained from the online archives of the Submillimeter Array ( SMA), a joint project between the Smithsonian Astrophysical Observatory and the Academia Sinica Institute of Astronomy and Astrophysics, funded by the Smithsonian Institution and the Academia Sinica. NR 29 TC 17 Z9 17 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD DEC 1 PY 2008 VL 688 IS 2 BP 852 EP 858 DI 10.1086/592138 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 373VU UT WOS:000261002400012 ER PT J AU Higdon, JL Higdon, SJU Willner, SP Brown, MJI Stern, D Le Floc'h, E Eisenhardt, P AF Higdon, J. L. Higdon, S. J. U. Willner, S. P. Brown, M. J. I. Stern, D. Le Floc'h, E. Eisenhardt, P. TI RADIO AND INFRARED SELECTED OPTICALLY INVISIBLE SOURCES IN THE BOOTES NDWFS SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: active; galaxies: high-redshift; galaxies: starburst; infrared: galaxies; radio continuum: galaxies ID SPITZER-SPACE-TELESCOPE; ACTIVE GALACTIC NUCLEI; SPECTRAL ENERGY-DISTRIBUTIONS; STAR-FORMATION HISTORY; HUBBLE DEEP FIELD; ARRAY CAMERA IRAC; HIGH-REDSHIFT; LUMINOUS GALAXIES; ELLIPTIC GALAXIES; FORMING GALAXIES AB We have combined data from the NOAO Deep Wide-Field Survey in Bootes and the Spitzer Space Telescope to determine basic properties for 16 optically "invisible'' MIPS 24 mu m and 35 optically invisible radio sources (OIMSs and OIRSs, respectively), including their spectral energy distributions (SEDs) and luminosities. Most OIMSs possess steep power-law SEDs over lambda(rest) = 1-10 mu m, indicating the presence of obscured AGNs in agreement with Spitzer spectroscopy. These objects are extremely luminous at rest-frame near- and mid-IR [vLv(5 mu m) approximate to 10(38)-10(39) W], consistent with accretion near the Eddington limit and further implying that they host buried QSOs. The majority of the IRAC-detected OIRSs have flat 3.6-24 mu m SEDs, implying comparable emission from stellar photospheres and hot AGN-illuminated dust. This may reflect relatively small amounts of dust close to the central engine or current low mass accretion rates. A small subset of OIRSs appear to be starburst-dominated with photometric redshifts from 1.0 to 4.5. The OIMSs and OIRSs with significant starburst components have similar L-K and stellar masses (M* approximate to 10(11) M-circle dot) assuming minimal AGN contribution. Roughly half of the OIRSs are not detected by Spitzer IRAC or MIPS. These are most likely z >= 2 radio galaxies. The IRAC-detected OIRSs are more likely than OIMSs to appear nonpointlike in the 3.6 and 4.5 mu m images, suggesting that interactions play a role in triggering their activity. The AGN-powered OIMSs may represent submillimeter galaxies making the transition from starburst to accretion dominance in their evolution to current-epoch massive ellipticals. C1 [Higdon, J. L.; Higdon, S. J. U.] Georgia So Univ, Dept Phys, Statesboro, GA 30460 USA. [Willner, S. P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Brown, M. J. I.] Monash Univ, Sch Phys, Clayton, Vic 3800, Australia. [Stern, D.; Eisenhardt, P.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Le Floc'h, E.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Le Floc'h, E.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. RP Higdon, JL (reprint author), Georgia So Univ, Dept Phys, Statesboro, GA 30460 USA. RI Brown, Michael/B-1181-2015 OI Brown, Michael/0000-0002-1207-9137 FU NASA through awards issued by JPL/Caltech; NASA/IPAC Extragalactic Database (NED); Jet Propulsion Laboratory; California Institute of Technology; National Aeronautics and Space Administration FX We wish to thank Terry Herter for valuable discussions relating to the template-fitting routines, as well as Julien Devriendt and Kevin Xu for access to their libraries of galaxy SEDs. We also wish to thank the anonymous referee for helpful suggestions and comments. 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. Support for this work was provided by NASA through awards issued by JPL/Caltech. 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. NR 69 TC 7 Z9 7 U1 0 U2 3 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD DEC 1 PY 2008 VL 688 IS 2 BP 885 EP 904 DI 10.1086/591069 PG 20 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 373VU UT WOS:000261002400015 ER PT J AU Trinchieri, G Pellegrini, S Fabbiano, G Fu, R Brassington, NJ Zezas, A Kim, DW Gallagher, J Angelini, L Davies, RL Kalogera, V King, AR Zepf, S AF Trinchieri, G. Pellegrini, S. Fabbiano, G. Fu, R. Brassington, N. J. Zezas, A. Kim, D. -W. Gallagher, J. Angelini, L. Davies, R. L. Kalogera, V. King, A. R. Zepf, S. TI DISCOVERY OF HOT GAS IN OUTFLOW IN NGC 3379 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: elliptical and lenticular, cD; galaxies: individual (NGC 3379); X-rays: galaxies; X-rays: ISM ID EARLY-TYPE GALAXIES; CCD SURFACE PHOTOMETRY; X-RAY-EMISSION; TO-LIGHT RATIO; ELLIPTIC GALAXIES; DARK-MATTER; STELLAR POPULATION; BLACK-HOLES; GLOBULAR-CLUSTERS; DEEP CHANDRA AB We report the discovery of a faint (L-X similar to 4 +/- 1.5 x 10(37) ergs s(-1), 0.5-2 keV), outflowing gaseous hot interstellar medium (ISM) in NGC 3379. This represents the lowest X-ray luminosity ever measured from a hot phase of the ISM in a nearby early-type galaxy. The discovery of the hot ISM in a very deep Chandra observation was possible thanks to its unique spectral and spatial signatures, which distinguish it from the integrated stellar X-ray emission, responsible for most of the unresolved emission in the Chandra data. This hot component is found in a region of similar to 800 pc in radius at the center of the galaxy and has a total mass M similar to 3 +/- 1 x 10(5) M-circle dot. Independent theoretical prediction of the characteristics of an ISM in this galaxy, based on the intrinsic properties of NGC 3379, reproduce well the observed luminosity, temperature, and radial distribution and mass of the hot gas, and indicate that the gas is in an outflowing phase, predicted by models but not observed in any system so far. C1 [Trinchieri, G.] Osserv Astron Brera, INAF, I-20212 Milan, Italy. [Pellegrini, S.] Univ Bologna, Dipartimento Astron, I-40127 Bologna, Italy. [Fabbiano, G.; Fu, R.; Brassington, N. J.; Zezas, A.; Kim, D. -W.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Gallagher, J.] Univ Wisconsin, Dept Astron, Madison, WI 53706 USA. [Angelini, L.] NASA, Goddard Space Flight Ctr, Lab Xray Astrophys, Greenbelt, MD 20771 USA. [Davies, R. L.] Univ Oxford, Subdept Astrophys, Oxford OX1 3RH, England. [Kalogera, V.] Northwestern Univ, Dept Phys & Astron, Evanston, IL 60208 USA. [King, A. R.] Univ Leicester, Theoret Astrophys Grp, Leicester LE1 7RH, Leics, England. [Zepf, S.] Michigan State Univ, Dept Phys & Astron, E Lansing, MI 48824 USA. RP Trinchieri, G (reprint author), Osserv Astron Brera, INAF, Via Brera 28, I-20212 Milan, Italy. EM ginevra.trinchieri@brera.inaf.it RI Zezas, Andreas/C-7543-2011; OI Zezas, Andreas/0000-0001-8952-676X; Trinchieri, Ginevra/0000-0002-0227-502X FU Chandra X-Ray Center (CXC) CIAO software and CALDB; SAOImage DS9; Smithsonian Astrophysical Observatory; Chandra GO [G06-7079A]; NASA LTSA [NAG5-13056]; Italian Space Agency ASI (Agenzia Spaziale Italiana) through grant ASI-INAF [I/023/05/0]; [NAS8-39073] FX We thank Stefano Andreon for many interesting discussions on the statistical aspects of the data analysis, and Terry Gaetz and Diab Jerius for their help in understanding the PSF issues. We thank the referee for raising the issue of the effects of the PSF, which prompted us to better investigate the reliability of the results. The data analysis was supported by the Chandra X-Ray Center (CXC) CIAO software and CALDB, and has made use of the SAOImage DS9 and funtools softwares, developed by the Smithsonian Astrophysical Observatory. We have used the NASA NED and ADS facilities, and have extracted archival data from the Chandra, HST, and 2MASS archives. This work was supported by the Chandra GO grant G06-7079A ( PI: G. Fabbiano) and subcontract G06-7079B ( PI: V. Kalogera). We acknowledge partial support from NASA contract NAS8-39073 (CXC); A. Zezas acknowledges support from NASA LTSA grant NAG5-13056; S. Pellegrini acknowledges partial financial support from the Italian Space Agency ASI (Agenzia Spaziale Italiana) through grant ASI-INAF I/023/05/0. NR 66 TC 22 Z9 22 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 DEC 1 PY 2008 VL 688 IS 2 BP 1000 EP 1008 DI 10.1086/592287 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 373VU UT WOS:000261002400022 ER PT J AU Abdo, AA Allen, B Aune, T Berley, D Blaufuss, E Casanova, S Chen, C Dingus, BL Ellsworth, RW Fleysher, L Fleysher, R Gonzalez, MM Goodman, JA Hoffman, CM Huntemeyer, PH Kolterman, BE Lansdell, CP Linnemann, JT McEnery, JE Mincer, AI Moskalenko, IV Nemethy, P Noyes, D Porter, TA Pretz, J Ryan, JM Parkinson, PMS Shoup, A Sinnis, G Smith, AJ Strong, AW Sullivan, GW Vasileiou, V Walker, GP Williams, DA Yodh, GB AF Abdo, A. A. Allen, B. Aune, T. Berley, D. Blaufuss, E. Casanova, S. Chen, C. Dingus, B. L. Ellsworth, R. W. Fleysher, L. Fleysher, R. Gonzalez, M. M. Goodman, J. A. Hoffman, C. M. Huentemeyer, P. H. Kolterman, B. E. Lansdell, C. P. Linnemann, J. T. McEnery, J. E. Mincer, A. I. Moskalenko, I. V. Nemethy, P. Noyes, D. Porter, T. A. Pretz, J. Ryan, J. M. Parkinson, P. M. Saz Shoup, A. Sinnis, G. Smith, A. J. Strong, A. W. Sullivan, G. W. Vasileiou, V. Walker, G. P. Williams, D. A. Yodh, G. B. TI MEASUREMENT OF THE SPATIAL DISTRIBUTION OF DIFFUSE TeV GAMMA-RAY EMISSION FROM THE GALACTIC PLANE WITH MILAGRO SO ASTROPHYSICAL JOURNAL LA English DT Article DE gamma rays: observations ID COSMIC-RAY; GALAXY; J2032+4130; DISCOVERY; SPECTRUM; CYGNUS; EXCESS; MATTER; RIDGE AB Diffuse gamma-ray emission produced by the interaction of cosmic-ray particles with matter and radiation in the Galaxy can be used to probe the distribution of cosmic rays and their sources in different regions of the Galaxy. With its large field of view and long observation time, the Milagro Gamma Ray Observatory is an ideal instrument for surveying large regions of the northern hemisphere sky and for detecting diffuse gamma-ray emission at very high energies. Here the spatial distribution and the flux of the diffuse gamma-ray emission in the TeV energy range with a median energy of 15 TeV for Galactic longitude between 30 degrees and 110 degrees and between 136 degrees and 216 degrees and for Galactic latitude between -10 degrees and 10 degrees are determined. The measured fluxes are consistent with predictions of the GALPROP model everywhere, except for the Cygnus region (l is an element of[65 degrees, 85 degrees]). For the Cygnus region, the flux is twice the predicted value. This excess can be explained by the presence of active cosmic-ray sources accelerating hadrons, which interact with the local dense interstellar medium and produce gamma rays through pion decay. C1 [Abdo, A. A.] USN, Res Lab, Washington, DC 20375 USA. [Allen, B.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Aune, T.; Porter, T. A.; Parkinson, P. M. Saz; Williams, D. A.] Univ Calif Santa Cruz, Santa Cruz, CA 95064 USA. [Berley, D.; Blaufuss, E.; Goodman, J. A.; Noyes, D.; Smith, A. J.; Sullivan, G. W.; Vasileiou, V.] Univ Maryland, College Pk, MD 20742 USA. [Casanova, S.] Max Planck Inst Kernphys, D-69117 Heidelberg, Germany. [Chen, C.; Yodh, G. B.] Univ Calif Irvine, Irvine, CA USA. [Dingus, B. L.; Hoffman, C. M.; Huentemeyer, P. H.; Pretz, J.; Sinnis, G.; Walker, G. P.] Los Alamos Natl Lab, Los Alamos, NM USA. [Ellsworth, R. W.] George Mason Univ, Fairfax, VA 22030 USA. [Fleysher, L.; Fleysher, R.; Kolterman, B. E.; Mincer, A. I.; Nemethy, P.] NYU, New York, NY USA. [Gonzalez, M. M.] Univ Nacl Autonoma Mexico, Inst Astron, Mexico City 04510, DF, Mexico. [Lansdell, C. P.] Inst Def Anal, Alexandria, VA USA. [Linnemann, J. T.] Michigan State Univ, E Lansing, MI 48824 USA. [McEnery, J. E.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Moskalenko, I. V.] Stanford Univ, HEPL, Stanford, CA 94305 USA. [Moskalenko, I. V.] Stanford Univ, KIPAC, Stanford, CA 94305 USA. [Ryan, J. M.] Univ New Hampshire, Durham, NH 03824 USA. [Shoup, A.] Ohio State Univ, Lima, OH 45804 USA. [Strong, A. W.] Max Planck Inst Extraterr Phys, D-37075 Garching, Germany. RP Abdo, AA (reprint author), USN, Res Lab, Washington, DC 20375 USA. RI McEnery, Julie/D-6612-2012; Casanova, Sabrina/J-8935-2013; Moskalenko, Igor/A-1301-2007; OI Casanova, Sabrina/0000-0002-6144-9122; Moskalenko, Igor/0000-0001-6141-458X; Dingus, Brenda/0000-0001-8451-7450 FU National Science Foundation [PHY-0245234, PHY-0302000, PHY-0400424, PHY-0504201, PHY-0601080, ATM-0002744]; Department of Energy (Office of High Energy Physics); Los Alamos National Laboratory; University of California; Institute for Geophysics and Planetary Physics at Los Alamos National Laboratory; NASA APRA FX We thank Scott Delay, Michael Schneider, and Owen Marshall for their dedicated efforts on the Milagro experiment. We also gratefully acknowledge the financial support of the National Science Foundation (under grants PHY-0245234, -0302000, -0400424, -0504201, -0601080, and ATM-0002744), the Department of Energy (Office of High Energy Physics), Los Alamos National Laboratory, the University of California, and the Institute for Geophysics and Planetary Physics at Los Alamos National Laboratory. I.V. Moskalenko acknowledges partial support from the NASA APRA grant. NR 35 TC 65 Z9 67 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD DEC 1 PY 2008 VL 688 IS 2 BP 1078 EP 1083 DI 10.1086/592213 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 373VU UT WOS:000261002400028 ER PT J AU Uchida, H Tsunemi, H Katsuda, S Kimura, M AF Uchida, Hiroyuki Tsunemi, Hiroshi Katsuda, Satoru Kimura, Masashi TI THE PLASMA STRUCTURE OF THE SOUTHWESTERN REGION OF THE CYGNUS LOOP WITH THE XMM-NEWTON OBSERVATORY SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM: abundances; ISM: individual (Cygnus Loop); supernova remnants; X-rays: ISM ID SUPERNOVA-REMNANTS; NORTHEASTERN RIM; NUCLEOSYNTHESIS; EXPLOSION; EMISSION; SUZAKU; FRONT AB We observed the southwestern region of the Cygnus Loop in two pointings with XMM-Newton. The region observed is called the "blow-out'' region, which is extended further in the south. The origin of the "blow out'' is not well understood, but it is suggested that there is another supernova remnant here in radio observation. To investigate in detail the structure of this region in X-ray, we divided our fields of view into 33 box regions. The spectra are well fitted by a two-component nonequilibrium ionization model. The emission measure distributions of heavy elements decrease from the inner region to the outer region of the Loop. Then, we also divided our fields of view into 26 annular sectors to examine the radial plasma structure. Judging from the metal abundances obtained, it is consistent that the X-ray emission is of Cygnus Loop origin, and we conclude that the high-kT(e) component (similar to 0.4 keV) originates from the ejecta, while the low-kT(e) component (similar to 0.2 keV) is derived from the swept-up interstellar medium. The flux of the low-kT(e) component is much less than that of high-kT(e) component, suggesting that the ISM component is very thin. Also, the relative abundances in the ejecta component show values similar to those obtained from previous observations of the Cygnus Loop. We find no evidence in X-ray that the nature of the "blow-out'' region originated from the extra supernova remnant. From the ejecta component, we calculated the masses for various metals and estimated the origin of the Cygnus Loop as a core-collapse explosion rather than a Type Ia supernova. C1 [Uchida, Hiroyuki; Tsunemi, Hiroshi; Katsuda, Satoru; Kimura, Masashi] Osaka Univ, Grad Sch Sci, Dept Earth & Space Sci, Osaka 5600043, Japan. [Katsuda, Satoru] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Uchida, H (reprint author), Osaka Univ, Grad Sch Sci, Dept Earth & Space Sci, Osaka 5600043, Japan. EM uchida@ess.sci.osaka-u.ac.jp; tsunemi@ess.sci.osaka-u.ac.jp; satoru.katsuda@nasa.gov; mkimura@ess.sci.osaka-u.ac.jp RI XRAY, SUZAKU/A-1808-2009 FU Ministry of Education, Culture, Sports, Science and Technology [16002004]; JSPS Research Fellowship for Young Scientists FX We thank H. Kosugi's careful reading of the manuscript. This work is partly supported by a Grant-in-Aid for Scientific Research by the Ministry of Education, Culture, Sports, Science and Technology (16002004). This study is also carried out as part of the 21st Century COE Program, "Towards a New Basic Science: Depth and Snthesis.'' H. U. and S. K. are supported by JSPS Research Fellowship for Young Scientists. NR 21 TC 11 Z9 11 U1 0 U2 2 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD DEC 1 PY 2008 VL 688 IS 2 BP 1102 EP 1111 DI 10.1086/592398 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 373VU UT WOS:000261002400030 ER PT J AU Bauer, FE Dwarkadas, VV Brandt, WN Immler, S Smartt, S Bartel, N Bietenholz, MF AF Bauer, F. E. Dwarkadas, V. V. Brandt, W. N. Immler, S. Smartt, S. Bartel, N. Bietenholz, M. F. TI SUPERNOVA 1996cr: SN 1987A's WILD COUSIN? SO ASTROPHYSICAL JOURNAL LA English DT Review DE circumstellar matter; supernovae: general; supernovae: individual (SN 1996cr); X-rays: individual (SN 1996cr) ID GAMMA-RAY BURST; RAPID PRESUPERNOVA EVOLUTION; WIND-DRIVEN BUBBLES; II SUPERNOVAE; CIRCUMSTELLAR MEDIUM; MASSIVE STARS; IA SUPERNOVA; RADIO OBSERVATIONS; CIRCINUS GALAXY; LIGHT ECHOES AB We report on new VLT optical spectroscopic and multiwavelength archival observations of SN 1996cr, a previously identified ultraluminous X-ray source known as Circinus galaxy X-2. Our optical spectrum confirms SN 1996cr as a bona fide Type IIn supernova, while archival imaging from the Anglo-Australian Telescope archive isolates the explosion date to between 1995 February 28 and 1996 March 16. SN 1996cr is one of the closest SNe (approximate to 3.8 Mpc) in the last several decades, and in terms of flux ranks among the brightest radio and X-ray SNe ever detected. The wealth of optical, X-ray, and radio observations that exist for this source provide relatively detailed constraints on its postexplosion expansion and progenitor history, including a preliminary angular size constraint from VLBI. Archival X-ray and radio data imply that the progenitor of SN 1996cr evacuated a large cavity just prior to exploding: the blast wave likely spent similar to 1-2 yr in relatively uninhibited expansion before eventually striking the dense circumstellar material which surrounds SN 1996cr. The X-ray and radio emission, which trace the progenitor mass-loss rate, have respectively risen by a factor of greater than or similar to 2 and remained roughly constant over the past 7 years. This behavior is reminiscent of the late rise of SN 1987A, but 1000 times more luminous and much more rapid to onset. SN 1996cr may likewise provide us with a younger example of SN 1978K and SN 1979C, both of which exhibit flat X-ray evolution at late times. Complex oxygen line emission hints at a possible concentric shell or ringlike structure. The discovery of SN 1996cr suggests that a substantial fraction of the closest SNe observed in the last several decades have occurred in wind-blown bubbles, and argues for the phenomena being widespread. C1 [Dwarkadas, V. V.] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA. [Brandt, W. N.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Immler, S.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Smartt, S.] Queens Univ Belfast, Sch Math & Phys, Astrophys Res Ctr, Belfast BT7 1NN, Antrim, North Ireland. [Bartel, N.; Bietenholz, M. F.] York Univ, Dept Phys & Astron, N York, ON M3J 1P3, Canada. [Bietenholz, M. F.] Hartebeesthoek Radio Observ, ZA-1740 Krugersdorp, South Africa. EM feb@astro.columbia.edu RI Brandt, William/N-2844-2015 OI Brandt, William/0000-0002-0167-2453 FU Chandra Postdoctoral Fellowship Award [PF4- 50032]; NSF award [AST- 0319261]; NASA STScI [HST- AR- 10649]; NASA LTSA [NAG5- 13035]; Leverhulme Trust; ESF EURYI scheme FX We thank Bjorn Emonts and Bryan Gaensler for help in reducing archival ATCA observations, Roger Chevalier, Claes Frannson, Dick McCray, Kurt Weiler, and Christopher Stockdale for useful discussions about the nature of the multiwavelength emission, Baerbel Koribalski for increasing our awareness of Australian online archives and access to proprietary ATCA observations, Ernesto Oliva and Alessandro Marconi for access to reduced NTT data, Bruno Leibundgut and Rob Fesen for their spectra of SN 1986J and SN 1979C, Philip Edwards, Steven Tingay, and Tasso Tzioumis for support of the VLBI observations, Kevin Hurley for directing us to revised IPN results which allowed us to reject an otherwise tentative GRB identification, John Raymond for helping to improve our emission- line tables, and the anonymous referee for useful comments that improved the content and presentation of the paper. We gratefully acknowledge the financial support of Chandra Postdoctoral Fellowship Award PF4- 50032 (F.E.B.), NSF award AST- 0319261 (V.V.D.), NASA STScI grant HST- AR- 10649 (V.V.D.), NASA LTSA grant NAG5- 13035 (W.N.B.), the Leverhulme Trust (S.J.S.) and the ESF EURYI scheme (S.J.S.). NR 134 TC 30 Z9 30 U1 0 U2 4 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD DEC 1 PY 2008 VL 688 IS 2 BP 1210 EP 1234 DI 10.1086/589761 PG 25 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 373VU UT WOS:000261002400039 ER PT J AU Bitner, MA Richter, MJ Lacy, JH Herczeg, GJ Greathouse, TK Jaffe, DT Salyk, C Blake, GA Hollenbach, DJ Doppmann, GW Najita, JR Currie, T AF Bitner, Martin A. Richter, Matthew J. Lacy, John H. Herczeg, Gregory J. Greathouse, Thomas K. Jaffe, Daniel T. Salyk, Colette Blake, Geoffrey A. Hollenbach, David J. Doppmann, Greg W. Najita, Joan R. Currie, Thayne TI THE TEXES SURVEY FOR H-2 EMISSION FROM PROTOPLANETARY DISKS SO ASTROPHYSICAL JOURNAL LA English DT Review DE circumstellar matter; infrared: stars; planetary systems: protoplanetary disks; stars: individual (AB Aur, DoAr 21, Elias 29, GSS 30 IRS 1, GV Tau N, HL Tau); stars: pre-main-sequence ID T-TAURI STARS; YOUNG STELLAR OBJECTS; MAIN-SEQUENCE STARS; MOLECULAR-HYDROGEN EMISSION; RHO-OPHIUCHI CLOUD; CO LINE EMISSION; SPACE-OBSERVATORY OBSERVATIONS; X-RAY OBSERVATIONS; HERBIG AE STARS; HIGH-RESOLUTION AB We report the results of a search for pure rotational molecular hydrogen emission from the circumstellar environments of young stellar objects with disks using the Texas Echelon Cross Echelle Spectrograph (TEXES) on the NASA Infrared Telescope Facility and the Gemini North Observatory. We searched for mid-infrared H-2 emission in the S(1), S(2), and S(4) transitions. Keck/NIRSPEC observations of the H-2 S(9) transition were included for some sources as an additional constraint on the gas temperature. We detected H-2 emission from 6 of 29 sources observed: AB Aur, DoAr 21, Elias 29, GSS 30 IRS 1, GV Tau N, and HL Tau. Four of the six targets with detected emission are class I sources that show evidence for surrounding material in an envelope in addition to a circumstellar disk. In these cases, we show that accretion shock heating is a plausible excitation mechanism. The detected emission lines are narrow (similar to 10 km s(-1)), centered at the stellar velocity, and spatially unresolved at scales of 0.4 '', which is consistent with origin from a disk at radii 10-50 AU from the star. In cases where we detect multiple emission lines, we derive temperatures greater than or similar to 500 K from similar to 1 M-circle plus of gas. Our upper limits for the nondetections place upper limits on the amount of H-2 gas with T > 500 K of less than a few Earth masses. Such warm gas temperatures are significantly higher than the equilibrium dust temperatures at these radii, suggesting that the gas is decoupled from the dust in the regions that we are studying and that processes such as UV, X-ray, and accretion heating may be important. C1 [Bitner, Martin A.; Lacy, John H.; Jaffe, Daniel T.] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA. [Richter, Matthew J.] Univ Calif Davis, Dept Phys, Davis, CA 95616 USA. [Herczeg, Gregory J.; Salyk, Colette; Blake, Geoffrey A.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. [Greathouse, Thomas K.] SW Res Inst, San Antonio, TX 78209 USA. [Hollenbach, David J.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Doppmann, Greg W.; Najita, Joan R.] Natl Opt Astron Observ, Tucson, AZ 85719 USA. [Currie, Thayne] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Bitner, MA (reprint author), Univ Texas Austin, Dept Astron, RLM 15308, Austin, TX 78712 USA. EM mbitner@astro.as.utexas.edu OI Greathouse, Thomas/0000-0001-6613-5731; Herczeg, Gregory/0000-0002-7154-6065 FU NSF [AST 06-07312, AST 07-08074]; NASA [NNG04GG92G] FX The authors wish to recognize and acknowledge the very significant cultural role and reverence that the summit of Mauna Kea has always had within the indigenous Hawaiian community. We are most fortunate to have the opportunity to conduct observations from this mountain. We thank the Gemini staff, and John White in particular, for their support of TEXES observations on Gemini North. The development of TEXES was supported by grants from the NSF and the NASA/USRA SOFIA project. Modification of TEXES for use on Gemini was supported by Gemini Observatory. Observations with TEXES were supported by NSF grant AST 06-07312. M.J.R. acknowledges support from NSF grant AST 07-08074 and NASA grant NNG04GG92G. 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. 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 Particle Physics and Astronomy Research Council (United Kingdom), the National Research Council (Canada), CONICYT (Chile), the Australian Research NR 145 TC 30 Z9 30 U1 0 U2 3 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD DEC 1 PY 2008 VL 688 IS 2 BP 1326 EP 1344 DI 10.1086/592317 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 373VU UT WOS:000261002400049 ER PT J AU Dodson-Robinson, SE Bodenheimer, P Laughlin, G Willacy, K Turner, NJ Beichman, CA AF Dodson-Robinson, Sarah E. Bodenheimer, Peter Laughlin, Gregory Willacy, Karen Turner, Neal J. Beichman, C. A. TI SATURN FORMS BY CORE ACCRETION IN 3.4 Myr SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE planets and satellites: formation; planets and satellites: individual (Saturn) ID GIANT PLANETS; OLIGARCHIC GROWTH; SOLAR-SYSTEM; JUPITER; MODELS; DISKS; GAS; PROTOPLANETS; CLOUD AB We present two new in situ core accretion simulations of Saturn with planet formation timescales of 3.37 Myr (model S0) and 3.48 Myr (model S1), consistent with observed protostellar disk lifetimes. In model S0, we assume rapid grain settling reduces opacity due to grains from full interstellar values. In model S1, we do not invoke grain settling, instead assigning full interstellar opacities to grains in the envelope. Surprisingly, the two models produce nearly identical formation timescales and core/atmosphere mass ratios. We therefore observe a new manifestation of core accretion theory: at large heliocentric distances, the solid core growth rate (limited by Keplerian orbital velocity) controls the planet formation timescale. We argue that this paradigm should apply to Uranus and Neptune as well. C1 [Dodson-Robinson, Sarah E.; Beichman, C. A.] CALTECH, NASA, Exoplanet Sci Inst, Pasadena, CA 91125 USA. [Bodenheimer, Peter; Laughlin, Gregory] Univ Calif Santa Cruz, Univ Calif Observ, Lick Observ, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA. [Willacy, Karen; Turner, Neal J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Dodson-Robinson, SE (reprint author), CALTECH, NASA, Exoplanet Sci Inst, 770 S Wilson Ave, Pasadena, CA 91125 USA. EM sdr@ipac.caltech.edu; chas@ipac.caltech.edu FU NSF Career [AST-0449986]; NASA Planetary Geology and Geophysics Program [NNG04GK19G]; NSF [AST-0507424]; NASA [NNX08AH82G]; National Aeronautics and Space Administration; JPL Research and Technology Development Program FX We thank Geoff Bryden and Jonathan Fortney for helpful conversations and the anonymous referee for suggesting model S1. This research was supported by a scholarship award from the Achievement Rewards for College Scientists Foundation to S. D. R.; by NSF Career Grant AST-0449986 and NASA Planetary Geology and Geophysics Program Grant NNG04GK19G to G. L.; and by NSF Grant AST-0507424 and NASA Origins Grant NNX08AH82G to P. B. The work of K. W. and N. T. was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration, with funding provided by the JPL Research and Technology Development Program. NR 28 TC 31 Z9 31 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD DEC 1 PY 2008 VL 688 IS 2 BP L99 EP L102 DI 10.1086/595616 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 398LG UT WOS:000262733000011 ER PT J AU Jess, DB Mathioudakis, M Crockett, PJ Keenan, FP AF Jess, D. B. Mathioudakis, M. Crockett, P. J. Keenan, F. P. TI DO ALL FLARES HAVE WHITE-LIGHT EMISSION? SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE Sun: activity; Sun: evolution; Sun: flares; Sun: photosphere; sunspots ID CONTINUUM EMISSION; INFRARED CONTINUUM; TRANSITION-REGION; CORONAL-EXPLORER; SOLAR-FLARES; YOHKOH; RESOLUTION; TELESCOPE; SUNSPOTS; HINODE AB High-cadence, multiwavelength optical observations of a solar active region (NOAA AR 10969), obtained with the Swedish Solar Telescope, are presented. Difference imaging of white light continuum data reveals a white-light brightening, 2 minutes in duration, linked to a cotemporal and cospatial C2.0 flare event. The flare kernel observed in the white-light images has a diameter of 300 km, thus rendering it below the resolution limit of most space-based telescopes. Continuum emission is present only during the impulsive stage of the flare, with the effects of chromospheric emission subsequently delayed by approximate to 2 minutes. The localized flare emission peaks at 300% above the quiescent flux. This large, yet tightly confined, increase in emission is only resolvable due to the high spatial resolution of the Swedish Solar Telescope. An investigation of the line-of-sight magnetic field derived from simultaneous MDI data shows that the continuum brightening is located very close to a magnetic polarity inversion line. In addition, an Ha flare ribbon is directed along a region of rapid magnetic energy change, with the footpoints of the ribbon remaining cospatial with the observed white-light brightening throughout the duration of the flare. The observed flare parameters are compared with current observations and theoretical models for M- and X-class events and we determine the observed white-light emission is caused by radiative back-warming. We suggest that the creation of white-light emission is a common feature of all solar flares. C1 [Jess, D. B.; Mathioudakis, M.; Crockett, P. J.; Keenan, F. P.] Queens Univ Belfast, Sch Math & Phys, Astrophys Res Ctr, Belfast BT7 1NN, Antrim, North Ireland. [Jess, D. B.] NASA, Goddard Space Flight Ctr, Solar Phys Lab, Greenbelt, MD 20771 USA. RP Jess, DB (reprint author), Queens Univ Belfast, Sch Math & Phys, Astrophys Res Ctr, Belfast BT7 1NN, Antrim, North Ireland. EM djess01@qub.ac.uk FU Northern Ireland Department for Employment and Learning studentship; Optical Infrared Coordination network (OPTICON); Research Infrastructures Programme of the European Commissions Sixth Framework Programme FX D. B. J. is supported by a Northern Ireland Department for Employment and Learning studentship. D. B. J. additionally thanks NASA Goddard Space Flight Center for a CAST studentship. F. P. K. is grateful to A. W. E. Aldermaston for the award of aWilliam Penney Fellowship. The Swedish 1 m Solar Telescope is operated on the island of La Palma by the Institute for Solar Physics of the Royal Swedish Academy of Sciences in the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofisica de Canarias. These observations have been funded by the Optical Infrared Coordination network (OPTICON), a major international collaboration supported by the Research Infrastructures Programme of the European Commissions Sixth Framework Programme. NR 33 TC 50 Z9 50 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD DEC 1 PY 2008 VL 688 IS 2 BP L119 EP L122 DI 10.1086/595588 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 398LG UT WOS:000262733000016 ER PT J AU Velusamy, T Peng, R Li, D Goldsmith, PF Langer, WD AF Velusamy, T. Peng, R. Li, D. Goldsmith, P. F. Langer, William D. TI DICHOTOMY IN THE DYNAMICAL STATUS OF MASSIVE CORES IN ORION SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE ISM: clouds; ISM: individual (Orion); ISM: kinematics and dynamics; ISM: molecules; stars: formation ID PROTOSTELLAR COLLAPSE; STARLESS CORES; QUIESCENT CORES; INFALL MOTIONS; LINE-PROFILES; CLOUD CORES; OBJECTS; SEARCH; STARS; B335 AB To study the evolution of high-mass cores, we have searched for evidence of collapse motions in a large sample of starless cores in the Orion molecular cloud. We used the Caltech Submillimeter Observatory telescope to obtain spectra of the optically thin (H(13)CO(+)) and optically thick (HCO(+)) high-density tracer molecules in 27 cores with masses >1 M(circle dot). The red-and blue-asymmetries seen in the line profiles of the optically thick line, with respect to the optically thin line indicate that 2/3 of these cores are not static. We detect evidence for infall (inward motions) in 9 cores and outward motions for 10 cores, suggesting a dichotomy in the kinematic state of the nonstatic cores in this sample. Our results provide an important observational constraint on the fraction of collapsing (inward motions) versus noncollapsing (reexpanding) cores for comparison with model simulations. C1 [Velusamy, T.; Li, D.; Goldsmith, P. F.; Langer, William D.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Peng, R.] Caltech Submillimeter Observ, Hilo, HI 96720 USA. RP Velusamy, T (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM Velusamy@jpl.nasa.gov; peng@submm.caltech.edu RI Goldsmith, Paul/H-3159-2016 FU NASA Astronomy and Physics Research and Analysis Program; NSF [AST-0229008] FX Letter was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration and supported by a grant from NASA Astronomy and Physics Research and Analysis Program. Research at the Caltech Submillimeter Observatory is supported by NSF grant AST-0229008. NR 21 TC 13 Z9 13 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD DEC 1 PY 2008 VL 688 IS 2 BP L87 EP L90 DI 10.1086/595585 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 398LG UT WOS:000262733000008 ER EF