FN Thomson Reuters Web of Science™ VR 1.0 PT J AU Dwek, E Arendt, RG Bouchet, P Burrows, DN Challis, P Danziger, IJ De Buizer, JM Gehrz, RD Kirshner, RP McCray, R Park, S Polomski, EF Woodward, CE AF Dwek, Eli Arendt, Richard G. Bouchet, Patrice Burrows, David N. Challis, Peter Danziger, I. John De Buizer, James M. Gehrz, Robert D. Kirshner, Robert P. McCray, Richard Park, Sangwook Polomski, Elisha F. Woodward, Charles E. TI Infrared and X-ray evidence for circumstellar grain destruction by the blast wave of supernova 1987A SO ASTROPHYSICAL JOURNAL LA English DT Article DE dust, extinction; infrared : general; ISM : individual (SNR 1987A); supernova remnants; X-rays : general ID SPITZER-SPACE-TELESCOPE; LARGE-MAGELLANIC-CLOUD; SN 1987A; CHANDRA OBSERVATIONS; REMNANT 1987A; DUST; EMISSION; SN-1987A; SPECTROGRAPH; ENVIRONMENT AB Multiwavelength observations of supernova remnant 1987A show that its morphology and luminosity are rapidly changing at X-ray, optical, infrared (IR), and radio wavelengths as the blast wave from the explosion expands into the circumstellar equatorial ring, produced by mass loss from the progenitor star. The observed IR radiation arises from the interaction of dust grains that formed in mass outflow with the soft X-ray-emitting plasma component of the shocked gas. Spitzer Infrared Spectrograph spectra at 5-30 mu m taken on day 6190 since the explosion show that the emission arises from similar to 1.1 x 10(-6) M-circle dot of silicate grains radiating at a temperature of similar to 180(-15)(+20) K. Subsequent observations on day 7137 show that the IR flux had increased by a factor of 2 while maintaining an almost identical spectral shape. The observed IR-to-X-ray flux ratio (IRX) is consistent with that of a dusty plasma with standard Large Magellanic Cloud dust abundances. IRX has decreased by a factor of similar to 2 between days 6190 and 7137, providing the first direct observation of the ongoing destruction of dust in an expanding supernova blast wave on dynamic timescales. Detailed models consistent with the observed dust temperature, the ionization timescale of the soft X-ray emission component, and the evolution of IRX suggest that the radiating silicate grains are immersed in a 3.5 x 10(6) K plasma with a density of (0.3-1) x 10(4) cm(-3) and have a size distribution that is confined to a narrow range of radii between 0.023 and 0.22 mu m. Smaller grains may have been evaporated by the initial UV flash from the supernova. C1 [Dwek, Eli] NASA, Goddard Space Flight Ctr, Observ Cosmol Lab, Greenbelt, MD 20771 USA. [Arendt, Richard G.] NASA, Goddard Space Flight Ctr, SSAI, Greenbelt, MD 20771 USA. [Bouchet, Patrice] CEA Saclay, Serv Astrophys, DSM, DAPNIA, F-91191 Gif Sur Yvette, France. [Burrows, David N.] Penn State Univ, Dept Astron & Astrophys, Davey Lab 525, University Pk, PA 16802 USA. [Challis, Peter; Kirshner, Robert P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Danziger, I. John] Osserv Astron Trieste, I-34131 Trieste, Italy. [De Buizer, James M.] So Operat Ctr, Gemini Observ, La Serena, Chile. [Gehrz, Robert D.; Polomski, Elisha F.; Woodward, Charles E.] Univ Minnesota, Dept Astron, Minneapolis, MN 55455 USA. [McCray, Richard] Univ Colorado, Joint Inst Lab Astrophys, Boulder, CO 80309 USA. RP Dwek, E (reprint author), NASA, Goddard Space Flight Ctr, Observ Cosmol Lab, Code 665, Greenbelt, MD 20771 USA. EM eli.dwek@nasa.gov; Patrice.Bouchet@cea.fr RI Dwek, Eli/C-3995-2012; OI Arendt, Richard/0000-0001-8403-8548 NR 30 TC 44 Z9 44 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 APR 1 PY 2008 VL 676 IS 2 BP 1029 EP 1039 DI 10.1086/529038 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 281WW UT WOS:000254530600020 ER PT J AU Thejappa, G MacDowall, RJ AF Thejappa, G. MacDowall, R. J. TI Effects of scattering on radio emission from the quiet Sun at low frequencies SO ASTROPHYSICAL JOURNAL LA English DT Article DE radio continuum : solar system; Sun : corona ID INNER SOLAR-WIND; CORONAL SCATTERING; LARGE-SCALE; DECAMETER WAVELENGTHS; DENSITY-FLUCTUATIONS; PLASMA FREQUENCY; TURBULENCE; RADIATION; SPECTRUM; METER AB The observations of the quiet Sun at meter and decameter wavelengths show that its brightness temperatures can be similar to 1 order of magnitude lower than the expected values of 10(6) K and the apparent diameters can be very large. We examine whether this unusual behavior is due to refraction in the smoothly varying coronal plasma and scattering by random density fluctuations using an improved Monte Carlo simulation technique. We use a three-dimensional model for the electron density, N-e, and a power-law spectrum for the density fluctuations with an exponential index of alpha. We consider two cases: (1) alpha = 11/3 (Kolmogorov spectrum), relative level of density fluctuations epsilon = Delta N-e/Ne = 0.1, and scale heights ranging from the inner scale l(i) = 684(N-e cm(-3))(-1/2) to outer scale l(o) = 10(6)l(i), and (2)alpha = 3 (flat spectrum), epsilon = 0.02, and scale heights ranging from 50 to 75 km. We consider the fluctuations to be anisotropic with axial ratios of similar to 10. The Kolmogorov type of fluctuations yield slightly lower brightness temperatures in comparison with those of a flat spectrum. The brightness temperature distributions, east-west diameters, and central brightness temperatures at various frequencies indicate that the refraction and scattering are probably the underlying reasons for the unusual behavior of the quiet-Sun radio emission. This study clearly demonstrates that Monte Carlo techniques can be very effective in extracting the coronal electron temperatures accurately from the radio data, provided the information about the density distributions and density fluctuations is known by some independent methods. C1 [Thejappa, G.] Univ Maryland, Dept Astron, College Pk, MD 20716 USA. [MacDowall, R. J.] NASA, Goddard Space Flight Ctr, College Pk, MD 20742 USA. RP Thejappa, G (reprint author), Univ Maryland, Dept Astron, College Pk, MD 20716 USA. EM thejappa@astro.umd.edu; robert.macdowall@nasa.gov RI MacDowall, Robert/D-2773-2012 NR 51 TC 25 Z9 25 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 APR 1 PY 2008 VL 676 IS 2 BP 1338 EP 1345 DI 10.1086/528835 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 281WW UT WOS:000254530600048 ER PT J AU Sabbi, E Gallagher, JS Smith, LJ De Mello, DF Mountain, M AF Sabbi, E. Gallagher, J. S. Smith, L. J. De Mello, D. F. Mountain, M. TI Holmberg IX: The nearest young galaxy SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE galaxies : evolution; galaxies : individual (Holmberg IX); galaxies : interactions; galaxies : photometry ID DWARF GALAXIES; STAR-FORMATION; NEUTRAL-HYDROGEN; M81 GROUP; SURFACE PHOTOMETRY; IRREGULAR GALAXIES; HI SURVEY; BRIDGE AB We present a study of the M81 companion dwarf irregular galaxy Holmberg IX using deep images taken with the Wide Field Channel of the Advanced Camera for Surveys on board the Hubble Space Telescope. Based on color-magnitude diagrams the resolved stellar population toward Holmberg IX contains numerous stars with ages of <= 200 Myr as well as older red giant stars. By charting the spatial distribution of the red giant stars and considering their inferred metallicities, we conclude that most of these older stars are associated with M81 or its tidal debris. At least 20% of the stellar mass in Holmberg IX was produced in the last similar to 200 Myr, giving it the youngest stellar population of any nearby galaxy. The location of Holmberg IX, its high gas content, and its youthful stellar population suggest that it is a tidal dwarf galaxy, perhaps formed during the last close passage of M82 around M81. C1 [Sabbi, E.; Smith, L. J.; Mountain, M.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Sabbi, E.] Univ Heidelberg, Zentrum Astron, Astron Rechen Inst, Heidelberg, Germany. [Sabbi, E.; Smith, L. J.] European Space Agcy, Res & Sci Support Dept, Baltimore, MD 21218 USA. [Gallagher, J. S.] Univ Wisconsin, Dept Astron, Madison, WI 53706 USA. [Smith, L. J.] UCL, Dept Phys & Astron, London WC1E 6BT, England. [De Mello, D. F.] NASA, Goddard Space Flight Ctr, Observat Cosmol Lab, Greenbelt, MD 20771 USA. [De Mello, D. F.] Catholic Univ Amer, Washington, DC 20064 USA. [De Mello, D. F.] Johns Hopkins Univ, Baltimore, MD 21218 USA. RP Sabbi, E (reprint author), Space Telescope Sci Inst, 3700 San Martin Dr, Baltimore, MD 21218 USA. NR 30 TC 24 Z9 24 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 APR 1 PY 2008 VL 676 IS 2 BP L113 EP L117 DI 10.1086/587548 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 291ZK UT WOS:000255235900006 ER PT J AU Dodson, R Fomalont, EB Wiik, K Horiuchi, S Hirabayashi, H Edwards, PG Murata, Y Asaki, Y Moellenbrock, GA Scott, WK Taylor, AR Gurvits, LI Paragi, Z Frey, S Shen, ZQ Lovell, JEJ Tingay, SJ Rioja, MJ Fodor, S Lister, ML Mosoni, L Coldwell, G Piner, BG Yang, J AF Dodson, R. Fomalont, E. B. Wiik, K. Horiuchi, S. Hirabayashi, H. Edwards, P. G. Murata, Y. Asaki, Y. Moellenbrock, G. A. Scott, W. K. Taylor, A. R. Gurvits, L. I. Paragi, Z. Frey, S. Shen, Z. -Q. Lovell, J. E. J. Tingay, S. J. Rioja, M. J. Fodor, S. Lister, M. L. Mosoni, L. Coldwell, G. Piner, B. G. Yang, J. TI The VSOP 5 GHz active galactic nucleus survey. V. Imaging results for the remaining 140 sources SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE galaxies : active; radio continuum : galaxies; surveys ID REFERENCE FRAME SOURCES; EXTRAGALACTIC RADIO-SOURCES; HEMISPHERE ICRF SOURCES; VLBA OBSERVATIONS; SPACE VLBI; ASTROMETRIC SUITABILITY; TEMPERATURE DISTRIBUTION; SCALE STRUCTURE; AGN SURVEY; QUASARS AB In 1997 February, the Japanese radio astronomy satellite HALCA was launched to provide the space-bourne element for the VLBI Space Observatory Program (VSOP) mission. Approximately 25% of the mission time was dedicated to the VSOP survey of bright compact active galactic nuclei (AGNs) at 5 GHz. This paper, the fifth in the series, presents images and models for the remaining 140 sources not included in the third paper in the series, which contained 102 sources. For most sources, the plots of the (u, v) coverage, the visibility amplitude versus (u, v) distance, and the high-resolution image are presented. Model fit parameters to the major radio components are determined, and the brightness temperature of the core component for each source is calculated. The brightness temperature distributions for all of the sources in the VSOP AGN survey are discussed. C1 [Dodson, R.; Wiik, K.; Hirabayashi, H.; Edwards, P. G.; Murata, Y.; Asaki, Y.; Moellenbrock, G. A.; Shen, Z. -Q.; Lovell, J. E. J.] Japan Aerosp Explorat Agcy, Inst Space & Astronaut Sci, Sagamihara, Kanagawa 2298510, Japan. [Dodson, R.; Rioja, M. J.] Observ Astron Nacl, E-28803 Alcala De Henares, Spain. [Fomalont, E. B.] Natl Radio Astron Observ, Charlottesville, VA 22903 USA. [Wiik, K.] Univ Turku, Tuorla Observ, FIN-21500 Piikkio, Finland. [Horiuchi, S.] Natl Astron Observ, Mitaka, Tokyo 1818588, Japan. [Horiuchi, S.; Tingay, S. J.; Fodor, S.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Horiuchi, S.; Tingay, S. J.] Swinburne Univ Technol, Ctr Astrophys & Supercomp, Hawthorn, Vic 3122, Australia. [Horiuchi, S.] Canberra Deep Space Commun Complex, Tuggeranong, ACT 2901, Australia. [Hirabayashi, H.; Murata, Y.; Asaki, Y.] Grad Univ Adv Studies, Sch Phys Sci, Dept Space & Astronaut Sci, Sagamihara, Kanagawa 2298510, Japan. [Edwards, P. G.; Lovell, J. E. J.] Commonwealth Sci & Ind Res Org, Australia Telescope Natl Facil, Epping, NSW 2122, Australia. [Moellenbrock, G. A.] Natl Radio Astron Observ, Socorro, NM 87801 USA. [Scott, W. K.; Taylor, A. R.] Univ Calgary, Dept Phys & Astron, Calgary, AB T2N 1N4, Canada. [Gurvits, L. I.; Paragi, Z.; Yang, J.] Joint Inst VLBI Europe, NL-7990 AA Dwingeloo, Netherlands. [Frey, S.; Mosoni, L.] FOMI Satellite Geodet Observ, H-1521 Budapest, Hungary. [Shen, Z. -Q.; Yang, J.] Chinese Acad Sci, Shanghai Astron Observ, Shanghai 200030, Peoples R China. [Paragi, Z.; Frey, S.] MTA Res Grp Phys Geodesy & Geodynam, H-1521 Budapest, Hungary. [Lovell, J. E. J.] Univ Tasmania, Sch Math & Phys, Hobart, Tas, Australia. [Tingay, S. J.] Curtin Univ Technol, Dept Imaging & Appl Phys, Perth, WA, Australia. [Fodor, S.; Piner, B. G.] Whittier Coll, Dept Phys, Whittier, CA 90608 USA. [Lister, M. L.] Purdue Univ, Dept Phys, W Lafayette, IN 47907 USA. [Mosoni, L.] MTA Konkoly Observ, H-1525 Budapest, Hungary. [Coldwell, G.] Univ Nacl Cordoba, Astron Observ, RA-5000 Cordoba, Argentina. RP Dodson, R (reprint author), Japan Aerosp Explorat Agcy, Inst Space & Astronaut Sci, 3-1-1 Yoshinodai, Sagamihara, Kanagawa 2298510, Japan. RI Tingay, Steven/B-5271-2013; Frey, Sandor/G-4465-2013 OI Frey, Sandor/0000-0003-3079-1889 NR 41 TC 25 Z9 25 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0067-0049 J9 ASTROPHYS J SUPPL S JI Astrophys. J. Suppl. Ser. PD APR PY 2008 VL 175 IS 2 BP 314 EP 355 DI 10.1086/525025 PG 42 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 327WN UT WOS:000257759300002 ER PT J AU Eisele, F Davis, DD Helmig, D Oltmans, SJ Neff, W Huey, G Tanner, D Chen, G Crawford, J Arimoto, R Buhr, M Mauldin, L Hutterli, M Dibb, J Blake, D Brooks, SB Johnson, B Roberts, JM Wang, YH Tan, D Flocke, F AF Eisele, Fred Davis, Douglas D. Helmig, Detlev Oltmans, Samuel J. Neff, William Huey, Greg Tanner, David Chen, Gao Crawford, Jim Arimoto, Richard Buhr, Martin Mauldin, Lee Hutterli, Manuel Dibb, Jack Blake, D. Brooks, Steven B. Johnson, Bryan Roberts, James M. Wang, Yuhang Tan, David Flocke, Frank TI Antarctic Tropospheric Chemistry Investigation (ANTCI) 2003 overview SO ATMOSPHERIC ENVIRONMENT LA English DT Editorial Material DE antarctic photochemistry; south pole chemistry; nitric oxide; hydroxyl radical; ozone ID 8 GLACIAL CYCLES; ICE-CORE; SOUTH-POLE; METHANESULFONATE; DIMETHYLSULFIDE; RECORD; FLUX AB The Antarctic Tropospheric Chemistry Investigation (ANTCI) was carried out from late November to December 2003 with both extended ground-based and tethered balloon studies at Amundsen Scott Station, South Pole. ANTCI 2003 was the first of two Antarctic field studies with the primary goal of further exploring the active photochemistry of the South Pole region that was first identified in the previous Investigation of Sulfur Chemistry in the Antarctic Troposphere (ISCAT) program. Since ISCAT was fully ground-based, ANTCI 2003 goals included expanding chemical studies both vertically upward to investigate mixing and horizontally to better understand large-scale plateau NO, production and transport. Thus, in addition to ground-based experiments at South Pole, Twin Otter aircraft sampling took place out to hundreds of kilometers in several directions from the South Pole. These were designed to specifically address the issue of how representative past South Pole chemical measurements are of the surrounding high plateau region. The Twin Otterwas also used to make transects along the coast both north and south of McMurdo Station. The present paper summarizes the overall setting and results of this investigation and highlights the many new findings that were obtained. (C) 2007 Elsevier Ltd. All rights reserved. C1 [Eisele, Fred; Flocke, Frank] Natl Ctr Atm Res, Atm Chem Div, Boulder, CO 80305 USA. [Eisele, Fred; Davis, Douglas D.; Huey, Greg; Tanner, David; Wang, Yuhang; Tan, David] Georgia Inst Technol, Sch Earth & Atm Sci, Atlanta, GA 30332 USA. [Helmig, Detlev] Univ Colorado, INSTAAR, Boulder, CO 80309 USA. [Oltmans, Samuel J.; Neff, William; Roberts, James M.] NOAA, Earth Syst Res Lab, Boulder, CO 80305 USA. [Chen, Gao; Crawford, Jim] NASA, Langley Res Ctr, Atm Sci Div, Hampton, VA 23681 USA. [Arimoto, Richard] New Mexico State Univ, Carlsbad Envir Monitoring Res Ctr, Carlsbad, NM 88220 USA. [Buhr, Martin] Air Qual Design Inc, Golden, CO 80403 USA. [Hutterli, Manuel] British Antarctic Survey, Cambridge CB3 0ET, England. [Hutterli, Manuel] Univ Arizona, Dept Hydrol & Water Resources, Tucson, AZ 85721 USA. [Dibb, Jack] Univ New Hampshire, Climate Change Res Ctr, Durham, NH 03824 USA. [Blake, D.] Univ Calif Irvine, Dept Chem, Irvine, CA 92717 USA. [Brooks, Steven B.] NOAA, Atmospher Turbulence & Diffus Div, Oak Ridge, TN USA. [Johnson, Bryan] NOAA, Syst Res Lab, Global Monitoring Div, Boulder, CO 80305 USA. RP Eisele, F (reprint author), Natl Ctr Atm Res, Atm Chem Div, Boulder, CO 80305 USA. EM eisele@ucar.edu RI Roberts, James/A-1082-2009; Crawford, James/L-6632-2013; Wang, Yuhang/B-5578-2014; Neff, William/E-2725-2010; Manager, CSD Publications/B-2789-2015 OI Roberts, James/0000-0002-8485-8172; Crawford, James/0000-0002-6982-0934; Neff, William/0000-0003-4047-7076; NR 28 TC 34 Z9 35 U1 0 U2 6 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 1352-2310 EI 1873-2844 J9 ATMOS ENVIRON JI Atmos. Environ. PD APR PY 2008 VL 42 IS 12 BP 2749 EP 2761 DI 10.1016/j.atmosenv.2007.04.013 PG 13 WC Environmental Sciences; Meteorology & Atmospheric Sciences SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences GA 314YS UT WOS:000256845700002 ER PT J AU Davis, DD Seelig, J Huey, G Crawford, J Chen, G Wang, YH Buhr, M Helmig, D Neff, W Blake, D Arimoto, R Eisele, F AF Davis, Douglas D. Seelig, Jon Huey, Greg Crawford, Jim Chen, Gao Wang, Yuhang Buhr, Marty Helmig, Detlev Neff, William Blake, Don Arimoto, Rich Eisele, Fred TI A reassessment of Antarctic plateau reactive nitrogen based on ANTO 2003 airborne and ground based measurements SO ATMOSPHERIC ENVIRONMENT LA English DT Article DE Antarctic plateau; reactive nitrogen; nitric oxide; airborne profiles; nitrate; recycling; hydroxyl radicals; oxidizing canopy; ice core chemical proxies ID FROZEN NITRATE SOLUTIONS; NEAR-SURFACE SNOW; SOUTH-POLE; BOUNDARY-LAYER; ICE CORES; PHOTOCHEMICAL PRODUCTION; ATMOSPHERIC CHEMISTRY; QUANTUM YIELDS; ACID; NOX AB The first airborne measurements of nitric oxide (NO) on the Antarctic plateau have demonstrated that the previously reported elevated levels of this species extend well beyond the immediate vicinity of South Pole. Although the current database is still relatively weak and critical laboratory experiments are still needed, the findings here suggest that the chemical uniqueness of the plateau may be substantially greater than first reported. For example, South Pole ground-based findings have provided new evidence showing that the dominant process driving the release of nitrogen from the snowpack during the spring/summer season (post-depositional loss) is photochemical in nature with evaporative processes playing a lesser role. There is also new evidence suggesting that nitrogen, in the form of nitrate, may undergo multiple recycling within a given photochemical season. Speculation here is that this may be a unique property of the plateau and much related to its having persistent cold temperatures even during summer. These conditions promote the efficient adsorption of molecules like HNO(3) (and very likely HO(2)NO(2)) onto snow-pack surface ice where we have hypothesized enhanced photochemical processing can occur, leading to the efficient release of NO(x) to the atmosphere. In addition, to these process-oriented tentative conclusions, the findings from the airborne studies, in conjunction with modeling exercises suggest a new paradigm for the plateau atmosphere. The near-surface atmosphere over this massive region can be viewed as serving as much more than a temporary reservoir or holding tank for imported chemical species. It defines an immense atmospheric chemical reactor which is capable of modifying the chemical characteristics of select atmospheric constituents. This reactor has most likely been in place over geological time, and may have led to the chemical modulation of some tracespecies now found in ice cores. Reactive nitrogen has played a critical role in both establishing and in maintaining this reactor. (C) 2007 Elsevier Ltd. All rights reserved. C1 [Davis, Douglas D.; Seelig, Jon; Huey, Greg; Wang, Yuhang] Georgia Inst Technol, Sch Earth & Atmospher Sci, Atlanta, GA 30332 USA. [Crawford, Jim; Chen, Gao] NASA, Langley Res Ctr, Hampton, VA 23681 USA. [Buhr, Marty] Air Qual Design, Golden, CO 80403 USA. [Helmig, Detlev] Univ Colorado, Inst Arctic & Alpine Res, Boulder, CO 80309 USA. [Neff, William] NOAA, Earth Syst Res Lab, Boulder, CO 80305 USA. [Blake, Don] Univ Calif Irvine, Dept Chem, Irvine, CA USA. [Arimoto, Rich] New Mexico State Univ, Carsbad Environm Monitoring & Res Ctr, Carlsbad, NM 88220 USA. [Eisele, Fred] Natl Ctr Atmospher Res, Div Atmospher Chem, Boulder, CO 80303 USA. RP Davis, DD (reprint author), Georgia Inst Technol, Sch Earth & Atmospher Sci, Atlanta, GA 30332 USA. EM douglas.davis@eas.gatech.edu RI Crawford, James/L-6632-2013; Wang, Yuhang/B-5578-2014; Neff, William/E-2725-2010 OI Crawford, James/0000-0002-6982-0934; Neff, William/0000-0003-4047-7076 NR 71 TC 46 Z9 48 U1 0 U2 12 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 1352-2310 J9 ATMOS ENVIRON JI Atmos. Environ. PD APR PY 2008 VL 42 IS 12 BP 2831 EP 2848 DI 10.1016/j.atmosenv.2007.07.039 PG 18 WC Environmental Sciences; Meteorology & Atmospheric Sciences SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences GA 314YS UT WOS:000256845700008 ER PT J AU Chambers, LH Alston, EJ Phelps, CS Moore, SW Diones, DD Oots, PC Fischer, JD Mims, FM AF Chambers, L. H. Alston, E. J. Phelps, C. S. Moore, S. W. Diones, D. D. Oots, P. C. Fischer, J. D. Mims, F. M., III TI The MY NASA DATA project SO BULLETIN OF THE AMERICAN METEOROLOGICAL SOCIETY LA English DT Article C1 [Chambers, L. H.; Alston, E. J.] NASA, Langley Res Ctr, Climate Sci Branch, Hampton, VA 23681 USA. [Phelps, C. S.; Moore, S. W.; Diones, D. D.; Oots, P. C.; Fischer, J. D.] Sci Applicat Int Corp, Hampton, VA USA. [Mims, F. M., III] Geronimo Creek Observ, Seguin, TX USA. RP Chambers, LH (reprint author), NASA, Langley Res Ctr, Climate Sci Branch, MS 420, Hampton, VA 23681 USA. EM l.h.chambers@larc.nasa.gov NR 1 TC 0 Z9 0 U1 0 U2 1 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 0003-0007 J9 B AM METEOROL SOC JI Bull. Amer. Meteorol. Soc. PD APR PY 2008 VL 89 IS 4 BP 437 EP 442 DI 10.1175/BAMS-89-4-437 PG 6 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 299YZ UT WOS:000255792800008 ER PT J AU Teixeira, J Stevens, B Bretherton, CS Cederwall, R Doyle, JD Golaz, JC Holtslag, AAM Klein, SA Lundquist, JK Randall, DA Siebesma, AR Soares, PMM AF Teixeira, J. Stevens, B. Bretherton, C. S. Cederwall, R. Doyle, J. D. Golaz, J. C. Holtslag, A. A. M. Klein, S. A. Lundquist, J. K. Randall, D. A. Siebesma, A. R. Soares, P. M. M. TI Parameterization of the atmospheric boundary layer SO BULLETIN OF THE AMERICAN METEOROLOGICAL SOCIETY LA English DT Article ID LARGE-EDDY SIMULATIONS C1 [Teixeira, J.] Naval Res Lab, Monterey, CA USA. [Teixeira, J.] NATO Undersea Res Ctr, La Spezia, Italy. [Stevens, B.] Univ Calif Los Angeles, Los Angeles, CA USA. [Bretherton, C. S.] Univ Washington, Seattle, WA 98195 USA. [Cederwall, R.; Klein, S. A.; Lundquist, J. K.] Lawrence Livermore Natl Lab, Livermore, CA USA. [Doyle, J. D.; Golaz, J. C.] USN, Res Lab, Monterey, CA USA. [Golaz, J. C.] Geophys Fluid Dynam Lab, Princeton, NJ USA. [Holtslag, A. A. M.] Wageningen Univ, Wageningen, Netherlands. [Randall, D. A.] Colorado State Univ, Ft Collins, CO 80523 USA. [Siebesma, A. R.] Royal Netherlands Meteorol Inst, NL-3730 AE De Bilt, Netherlands. [Soares, P. M. M.] Univ Lisbon, P-1699 Lisbon, Portugal. [Soares, P. M. M.] Inst Super Engn Lisboa, Lisbon, Portugal. RP Teixeira, J (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr,MS 169-237, Pasadena, CA 91109 USA. EM Teixeira@ipl.nasa.gov RI Randall, David/E-6113-2011; Soares, Pedro /K-6239-2012; Stevens, Bjorn/A-1757-2013; Golaz, Jean-Christophe/D-5007-2014; Klein, Stephen/H-4337-2016; Holtslag, Albert/B-7842-2010 OI Randall, David/0000-0001-6935-4112; Soares, Pedro /0000-0002-9155-5874; Stevens, Bjorn/0000-0003-3795-0475; Golaz, Jean-Christophe/0000-0003-1616-5435; Klein, Stephen/0000-0002-5476-858X; Holtslag, Albert/0000-0003-0995-2481 NR 7 TC 31 Z9 31 U1 1 U2 12 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 0003-0007 J9 B AM METEOROL SOC JI Bull. Amer. Meteorol. Soc. PD APR PY 2008 VL 89 IS 4 BP 453 EP 458 DI 10.1175/BAMS-89-4-453 PG 6 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 299YZ UT WOS:000255792800011 ER PT J AU Creilson, JK Pippin, MR Henderson, BL Ladd, IH Fishman, J Votapkova, D Krpcova, I AF Creilson, John K. Pippin, Margaret R. Henderson, Bryana L. Ladd, Irene H. Fishman, Jack Votapkova, Dana Krpcova, Ilona TI Surface ozone measured at globe schools in the Czech Republic - A demonstration of the importance of student contribution to the larger science picture SO BULLETIN OF THE AMERICAN METEOROLOGICAL SOCIETY LA English DT Article AB Global Learning and Observations to Benefit the Environment (GLOBE) is a worldwide, hands-on, primary and secondary school-based education and science program, which is developed to give students a chance to perform real science by making measurements, analyzing data, and participating in research through collaboration with scientists. As part of the GLOBE Surface Ozone of the TEREZA Association in the Czech Republic, schools in the Czech Republic have been making and reporting daily measurements of surface ozone and surface meteorological data since 2001. Using a hand-held ozone monitor developed for GLOBE, students at several Czech schools have generated multiyear data records of surface ozone from 2001 to 2005. Analysis of the data shows that surface ozone levels were anomalously high during the summer of 2003 relative to other summers. These findings are consistent with the measurements of the European Environment Agency, which highlight the summer of 2003 as having exceptionally long-lasting and spatially extensive episodes of high surface ozone, especially during the first half of August. Further analysis of the summer's prevailing meteorology shows not only that it was one of the hottest on record, a finding also. seen in the student data, but the conditions for production of ozone were ideal. Findings such as these increase student, teacher, and scientist confidence in the utility of the GLOBE data for engaging budding scientists in the collection, analysis, and eventual interpretation of the data for inquiry-based education. C1 [Creilson, John K.] John K Creilson Sci Syst & Applicat Inc, Hampton, VA 23666 USA. [Pippin, Margaret R.; Ladd, Irene H.; Fishman, Jack] NASA, Langley Res Ctr, Chem & Dynam Branch, Hampton, VA 23665 USA. [Henderson, Bryana L.] NASA, Langley Res Ctr, Langley Aerosp Res Summer Scholars Program, Hampton, VA 23665 USA. [Votapkova, Dana; Krpcova, Ilona] TEREZA Assoc, Prague, Czech Republic. RP Creilson, JK (reprint author), John K Creilson Sci Syst & Applicat Inc, 1 Enterprise Pkway,Suite 200, Hampton, VA 23666 USA. EM john.k.creilson@nasa.gov NR 16 TC 1 Z9 1 U1 1 U2 4 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 0003-0007 J9 B AM METEOROL SOC JI Bull. Amer. Meteorol. Soc. PD APR PY 2008 VL 89 IS 4 BP 505 EP + DI 10.1175/BAMS-89-4-505 PG 11 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 299YZ UT WOS:000255792800016 ER PT J AU Ferrick, MG Mulherin, ND Haehnel, RB Coutermarsh, BA Durell, GD Tantillo, TJ Curtis, LA Clair, TLS Weiser, ES Cano, RJ Smith, TM Martinez, EC AF Ferrick, M. G. Mulherin, N. D. Haehnel, R. B. Coutermarsh, B. A. Durell, G. D. Tantillo, T. J. Curtis, L. A. Clair, T. L. St. Weiser, E. S. Cano, R. J. Smith, T. M. Martinez, E. C. TI Evaluation of ice release coatings at cryogenic temperature for the space shuttle SO COLD REGIONS SCIENCE AND TECHNOLOGY LA English DT Article DE double lap shear testing; cryogenic temperatures; ice adhesion; ice phobic coatings; space shuttle AB The brackets that secure the liquid oxygen feed line to the external tank are known locations of frost and ice growth during the pre-launch period following fuel loading. This experimental program quantified the reduction in adhesion that resulted when ice phobic coatings were applied to test coupons that simulated the bracket surface. Double lap shear testing of coated and uncoated coupons provided robust test specimens and consistent load response patterns with exceptional resolution. Ice was grown as strong and consistently as possible for these tests and then subjected to temperature decreases comparable to those of the bracket. All tests were conducted at a constant temperature of -112 degrees C (-170 degrees F) and included uncoated controls with each group of samples. The program evolved in three phases. Phase I evaluated a wide range of coatings, and showed that Rain-X mixed with MP-55 powdered Teflon (RXM) was an outstanding coating to reduce ice adhesion to Koropon coated aluminum. Coating material retained on the ice surface following each test indicated failure in the coating and the potential for loss of effectiveness with repeated ice formation and release. Phase 2 evaluated modifications to RXM that might enhance durability while maintaining effectiveness. However, the modified mixtures did not improve coating durability or ice release. Phase 3 focused on the effects of mixing method, cure time, wiping off of excess coating, and coating resistance to weathering by water. A progressive coating loss again occurred through repeat test cycles, but performance generally improved. Results also indicated that cure times longer than 1.5 h prior to coating disturbance are needed for optimal performance. The MP-55 remaining on coupon surfaces after 3 cycles of testing and on one untested coupon from the same group was measured with XPS. The tested coupons retained slightly less MP-55 than the untested coupon, confirming the loss of coating. Contact angle analysis of these same coupons showed that the hydrophobic performance of the tested surfaces was largely preserved. Scanning electron microscopy with an energy dispersive spectroscopy elemental map indicated that the MP-55 was evenly dispersed throughout the coated surface, and abrasive wiping did not remove a significant portion of the Teflon. Test results suggest follow-up studies to refine the optimal coating formulation, mixing and application procedures, and understanding of reaction processes, cure time, and coating durability. Double lap shear testing and XPS analysis can quantify ice adhesion and coating profile thickness changes with cycling, and is capable of resolving these remaining issues. (c) 2007 Elsevier B.V. All rights reserved. C1 [Ferrick, M. G.; Mulherin, N. D.; Haehnel, R. B.; Coutermarsh, B. A.; Durell, G. D.; Tantillo, T. J.] USA, Cold Reg Res & Engn Lab, Engineer Res & Dev Ctr, Hanover, NH 03755 USA. [Clair, T. L. St.] Natl Inst Aerosp, Hampton, VA USA. [Weiser, E. S.; Cano, R. J.] NASA, Langley Res Ctr, Hampton, VA 23665 USA. [Smith, T. M.] NASA, John F Kennedy Space Ctr, KSC, Kennedy Space Ctr, FL 32899 USA. RP Ferrick, MG (reprint author), USA, Cold Reg Res & Engn Lab, Engineer Res & Dev Ctr, 72 Lyme Rd, Hanover, NH 03755 USA. EM michael.g.ferrick@crdc.usace.army.mil NR 5 TC 12 Z9 12 U1 3 U2 15 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0165-232X J9 COLD REG SCI TECHNOL JI Cold Reg. Sci. Tech. PD APR PY 2008 VL 52 IS 2 BP 224 EP 243 DI 10.1016/j.coldregions.2007.03.002 PG 20 WC Engineering, Environmental; Engineering, Civil; Geosciences, Multidisciplinary SC Engineering; Geology GA 291YX UT WOS:000255234600011 ER PT J AU Wahlgren, GM AF Wahlgren, G. M. TI Weak emission lines and peculiar stars SO CONTRIBUTIONS OF THE ASTRONOMICAL OBSERVATORY SKALNATE PLESO LA English DT Article; Proceedings Paper CT CP/AP Workshop 2007 CY SEP 10-14, 2007 CL Vienna, AUSTRIA SP House Cafe Eat, Univ Wien, Power Horse Energy Drink, Kultur Niederosterreich, Wien Kultur, MKS, Ltrock Brot, EDV Serv Doppler, Rosch Frisch, OGA, Comp Delphin, Bank Austria Creditanstalt, J Syst Em Tech, UniCredit Grp DE stars : B-type; stars : chemically peculiar; spectral lines : emission ID MAIN-SEQUENCE STARS; X-RAY-EMISSION; B-TYPE STARS; MNII EMISSION; SPECTRUM; CENTAURI; ANGSTROM; 3-CEN-A; ORIGIN AB Weak emission lines (WELs) of metals are observed in sharp-lined spectra of mid- to late-B type stars. The WELs are detected over a range of element abundance and are found among both chemically-normal and chemically-peculiar stars. The characteristics of this ubiquitous phenomenon are reviewed and their potential for the study of inhomogeneous stellar atmospheres is presented. C1 [Wahlgren, G. M.] Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA. [Wahlgren, G. M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Wahlgren, GM (reprint author), Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA. NR 18 TC 3 Z9 3 U1 0 U2 1 PU SLOVAK ACADEMY SCIENCES ASTRONOMICAL INST PI TATRANSKA LOMINICA PA SLOVAK ACADEMY SCIENCES ASTRONOMICAL INST, TATRANSKA LOMINICA, SK-059 60, SLOVAKIA SN 1335-1842 J9 CONTRIB ASTRON OBS S JI Contrib. Astron. Obs. S. PD APR PY 2008 VL 38 IS 2 BP 279 EP 284 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 310FJ UT WOS:000256514000028 ER PT J AU Wahlgren, GM Leckrone, DS AF Wahlgren, G. M. Leckrone, D. S. TI Heavy elements in the hot-Am star HR 3383 SO CONTRIBUTIONS OF THE ASTRONOMICAL OBSERVATORY SKALNATE PLESO LA English DT Article; Proceedings Paper CT CP/AP Workshop 2007 CY SEP 10-14, 2007 CL Vienna, AUSTRIA SP House Cafe Eat, Univ Wien, Power Horse Energy Drink, Kultur Niederosterreich, Wien Kultur, MKS, Ltrock Brot, EDV Serv Doppler, Rosch Frisch, OGA, Comp Delphin, Bank Austria Creditanstalt, J Syst Em Tech, UniCredit Grp DE stars : chemically peculiar; stars : abundances; techniques : spectroscopic; ultraviolet : stars AB The ultraviolet spectrum of the hot-Am star HR 3383 is analyzed through synthetic spectrum fitting for identification of lines from post iron-group elements. Spectral lines for a number of ions are detected for the first time in this star. C1 [Wahlgren, G. M.] Catholic Univ Amer, Washington, DC 20064 USA. [Wahlgren, G. M.; Leckrone, D. S.] NASA, Goddard Space Flight Ctr, Code 667, Greenbelt, MD 20771 USA. RP Wahlgren, GM (reprint author), Catholic Univ Amer, Washington, DC 20064 USA. NR 4 TC 2 Z9 2 U1 0 U2 1 PU SLOVAK ACADEMY SCIENCES ASTRONOMICAL INST PI TATRANSKA LOMINICA PA SLOVAK ACADEMY SCIENCES ASTRONOMICAL INST, TATRANSKA LOMINICA, SK-059 60, SLOVAKIA SN 1335-1842 J9 CONTRIB ASTRON OBS S JI Contrib. Astron. Obs. S. PD APR PY 2008 VL 38 IS 2 BP 463 EP 464 PG 2 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 310FJ UT WOS:000256514000078 ER PT J AU Harvey, CC Gangloff, M King, T Perry, CH Roberts, DA Thieman, JR AF Harvey, Christopher C. Gangloff, Michel King, Todd Perry, Christopher H. Roberts, D. Aaron Thieman, James R. TI Virtual observatories for space and solar physics research SO EARTH SCIENCE INFORMATICS LA English DT Review DE Datamodel; Interoperability; Solar system plasma; SPASE; Virtual observatory AB As soon as the first data became available online over the Internet, it was obvious that different sites holding related datasets should appear to the end user as a single data system, even if the data itself is stored at multiple locations. To achieve this objective in the context of continuing parallel development of multiple data centres, in 2003 several actors in the realm of space plasmas created the international consortium Space Physics Archive Search and Extract (SPASE). Since 2005 US participation in SPASE has been supported by NASA, and early in 2006 NASA funded five new Virtual Observatories to cater for different aspects of solar system plasma science. This paper outlines the current status of the SPASE effort, the opportunities it offers, its specificities with respect to other parts of the astronomical virtual observatory, and the possibilities it offers for space weather. C1 [Harvey, Christopher C.; Gangloff, Michel] CNRS CESR, Toulouse 04, France. [King, Todd] Univ Calif Los Angeles, UCLA IGPP, Los Angeles, CA 90024 USA. [Thieman, James R.] NASA, Goddard Space Flight Ctr, Sci & Explorat Directorate, NASA GSFC, Greenbelt, MD 20771 USA. [Perry, Christopher H.] Rutherford Appleton Lab, Didcot OX11 0WX, Oxon, England. RP Harvey, CC (reprint author), CNRS CESR, 9 Ave Colonel Roche,BP 4346, Toulouse 04, France. EM Harvey@cesr.fr; Gangloff@cesr.fr; tking@igpp.ucla.edu; C.H.Perry@rl.ac.uk; aaron.roberts@nasa.gov; james.r.thieman@nasa.gov NR 9 TC 3 Z9 3 U1 0 U2 1 PU SPRINGER HEIDELBERG PI HEIDELBERG PA TIERGARTENSTRASSE 17, D-69121 HEIDELBERG, GERMANY SN 1865-0473 J9 EARTH SCI INFORM JI Earth Sci. Inform. PD APR PY 2008 VL 1 IS 1 BP 5 EP 13 DI 10.1007/s12145-008-0008-1 PG 9 WC Computer Science, Interdisciplinary Applications; Geosciences, Multidisciplinary SC Computer Science; Geology GA V15EM UT WOS:000207785300003 ER PT J AU King, T Merka, J Walker, R Joy, S Narock, T AF King, Todd Merka, Jan Walker, Raymond Joy, Steven Narock, Tom TI The architecture of a multi-tiered virtual observatory SO EARTH SCIENCE INFORMATICS LA English DT Article DE Harvesting; Search registry; Topology; Virtual observatory AB Virtual observatories are being established in a wide range a disciplines, supported by a variety of agencies. Groups such as the International Virtual Observatory Alliance (IVOA), Planetary Data System (PDS) and the Space Physics Archive Search and Extract (SPASE) consortium are defining metadata standards to aid in archiving and sharing of information resources. The role of the virtual observatories in this resource sharing environment is to locate available resources and help users find the resources they need and then gain access to those resources. There are many different existing resource providers from which virtual observatories must collect descriptions of their resources. These resource providers may have associations with other providers so the topology of information exchange can be complicated. We explore the variety of topologies that can exist and discuss methods of collecting (harvesting) information from providers such as scheduled and on-demand harvesting. We compare the benefits of each approach and look at the issues of management overhead, adaptability and timeliness. We also explore the benefits of combining searching and harvesting services as part of a comprehensive solution. C1 [King, Todd; Walker, Raymond; Joy, Steven] Univ Calif Los Angeles, Inst Geophys & Planetary Phys, Los Angeles, CA 90024 USA. [Merka, Jan; Narock, Tom] Univ Maryland Baltimore Cty, Goddard Earth Sci & Technol Ctr, Baltimore, MD 21228 USA. [Merka, Jan; Narock, Tom] NASA, Goddard Space Flight Ctr, Heliospher Phys Lab, Greenbelt, MD 20771 USA. RP King, T (reprint author), Univ Calif Los Angeles, Inst Geophys & Planetary Phys, Los Angeles, CA 90024 USA. EM tking@igpp.ucla.edu OI Narock, Tom/0000-0002-9785-4496 FU National Aeronautics and Space Administration [NNX07AC95G, NNX07AC93G]; Virtual Observatories for Solar and Space Physics Data [S3CVO] FX This work was supported by the National Aeronautics and Space Administration under Grants No. NNX07AC95G and NNX07AC93G and issued through the Virtual Observatories for Solar and Space Physics Data (S3CVO). The UCLA/IGPP publication number is 6359. NR 13 TC 4 Z9 4 U1 0 U2 2 PU SPRINGER HEIDELBERG PI HEIDELBERG PA TIERGARTENSTRASSE 17, D-69121 HEIDELBERG, GERMANY SN 1865-0473 J9 EARTH SCI INFORM JI Earth Sci. Inform. PD APR PY 2008 VL 1 IS 1 BP 21 EP 28 DI 10.1007/s12145-008-0006-3 PG 8 WC Computer Science, Interdisciplinary Applications; Geosciences, Multidisciplinary SC Computer Science; Geology GA V15EM UT WOS:000207785300005 ER PT J AU King, T Narock, T Walker, R Merka, J Joy, S AF King, Todd Narock, Tom Walker, Raymond Merka, Jan Joy, Steven TI A brave new (virtual) world: distributed searches, relevance scoring and facets SO EARTH SCIENCE INFORMATICS LA English DT Article DE Relevance scoring facets virtual observatory search AB Our ability to deal with complex systems has improved through information system research which includes improved modeling (both data and system), the use of semantics and advances in distributed computing. The past decade has seen an explosion in the amount and variety of geosciences data and the emergence of true open data repositories through which scientists can freely access this data. Those data are found in thousands of repositories located around the world. Virtual observatories have been created to address the challenge of helping scientists search those repositories to find and access the required data. This challenge is been addressed by using technologies such as the Internet (with ample connectivity and bandwidth), the Web, cheap computing power, cheap storage and standards for critical components. Many scientific disciplines are developing virtual observatories. Yet some of the most compelling science questions cross multiple domains. While semantics can provide cross domain reasoning, often the first step in answering a question is determining what resources are available which may be relevant to a topic. The topic can be expressed as simple phrases or word sequences. Using a common relevance scoring method at all locations can enable a federated search across loosely coupled providers. The results of which can be organized into facets to aid the user in selecting the most promising resources with which to pursue the scientific investigation. We describe an approach to developing and deploying relevance scoring methods and faceted results in this brave new (virtual) world. We have found that a scoring method which considers both the presence of terms and the proximity of these terms relative to the order of the terms in the query improves the assessment of relevance. We call this Term Presence-Proximity (TPP) scoring and describe a method for calculating a normalized score. TPP scoring compares favorably with other scoring approaches. C1 [King, Todd; Walker, Raymond; Joy, Steven] Univ Calif Los Angeles, Inst Geophys & Planetary Phys, Los Angeles, CA 90024 USA. [Narock, Tom; Merka, Jan] Univ Maryland Baltimore Cty, Goddard Earth Sci & Technol Ctr, Baltimore, MD 21228 USA. [Narock, Tom; Merka, Jan] NASA, Goddard Space Flight Ctr, Heliospher Phys Lab, Greenbelt, MD 20771 USA. RP King, T (reprint author), Univ Calif Los Angeles, Inst Geophys & Planetary Phys, Los Angeles, CA 90024 USA. EM tking@igpp.ucla.edu FU National Aeronautics and Space Administration [NNX07AC95G, NNX07AC93G]; Virtual Observatories for Solar and Space Physics Data [S3CVO] FX This work was supported by the National Aeronautics and Space Administration under Grants No. NNX07AC95G and NNX07AC93G and issued through the Virtual Observatories for Solar and Space Physics Data (S3CVO). The UCLA/IGPP publication number is 6360. NR 10 TC 5 Z9 5 U1 0 U2 1 PU SPRINGER HEIDELBERG PI HEIDELBERG PA TIERGARTENSTRASSE 17, D-69121 HEIDELBERG, GERMANY SN 1865-0473 J9 EARTH SCI INFORM JI Earth Sci. Inform. PD APR PY 2008 VL 1 IS 1 BP 29 EP 34 DI 10.1007/s12145-008-0002-7 PG 6 WC Computer Science, Interdisciplinary Applications; Geosciences, Multidisciplinary SC Computer Science; Geology GA V15EM UT WOS:000207785300006 ER PT J AU Merka, J Narock, TW Szabo, A AF Merka, Jan Narock, Thomas W. Szabo, Adam TI Navigating through SPASE to heliospheric and magnetospheric data SO EARTH SCIENCE INFORMATICS LA English DT Article DE Middleware; SPASE metadata; VHO; Virtual observatory search; VMO AB Virtual observatories have been introduced by the astrophysics community as an environment connecting distributed data sources with a unified interface. The heliophysics community soon recognized that they faced a similar problem of many distributed data sets with varying amount of information about them and several discipline specific virtual observatories have been established. Two of them, the virtual heliospheric observatory (VHO) and the virtual magnetospheric observatory (VMO), share a common architecture design with development efforts oriented towards a structured data search. This paper describes the VHO/VMO middleware and its components from metadata preparation and processing to the user interface. C1 [Merka, Jan; Narock, Thomas W.] Univ Maryland, Goddard Earth Sci & Technol Ctr, Baltimore, MD 21201 USA. [Merka, Jan; Narock, Thomas W.; Szabo, Adam] NASA, Goddard Space Flight Ctr, Heliospher Phys Lab, Greenbelt, MD 20771 USA. RP Merka, J (reprint author), Univ Maryland, Goddard Earth Sci & Technol Ctr, Baltimore, MD 21201 USA. EM jan.merka@nasa.gov OI Narock, Tom/0000-0002-9785-4496 FU National Aeronautics and Space Administration [NNX07AC95G]; virtual observatories for Solar and Space Physics Data [S3CVO] FX This work was supported by the National Aeronautics and Space Administration under Grant No. NNX07AC95G issued through the virtual observatories for Solar and Space Physics Data (S3CVO). NR 9 TC 5 Z9 5 U1 0 U2 2 PU SPRINGER HEIDELBERG PI HEIDELBERG PA TIERGARTENSTRASSE 17, D-69121 HEIDELBERG, GERMANY SN 1865-0473 J9 EARTH SCI INFORM JI Earth Sci. Inform. PD APR PY 2008 VL 1 IS 1 BP 35 EP 42 DI 10.1007/s12145-008-0004-5 PG 8 WC Computer Science, Interdisciplinary Applications; Geosciences, Multidisciplinary SC Computer Science; Geology GA V15EM UT WOS:000207785300007 ER PT J AU Narock, TW King, T AF Narock, T. W. King, T. TI Developing a SPASE Query Language SO EARTH SCIENCE INFORMATICS LA English DT Article DE Virtual observatory; Data search; Data retrieval; Virtual observatory communication AB The advent of the Virtual Observatory has begun an evolution in the space physics data environment. A number of nascent and discipline specific Virtual Observatories have started to emerge with an emphasis on data search and retrieval. As this new data environment takes shape an emphasis will be placed on interdisciplinary communication in attempts to address large scale and global problems. To this end we formulate the development of a query language to facilitate Virtual Observatory to Virtual Observatory communication. Furthermore, we outline the goals of such a language, how it would work and how existing community efforts can be leveraged to speed the development of this query language. C1 [Narock, T. W.] Univ Maryland Baltimore Cty, Goddard Earth Sci & Technol Ctr, Baltimore, MD 21228 USA. [Narock, T. W.] NASA, Goddard Space Flight Ctr, Heliospher Phys Lab, Greenbelt, MD 20771 USA. [King, T.] Univ Calif Los Angeles, Inst Geophys & Planetary Phys, Los Angeles, CA 90024 USA. RP Narock, TW (reprint author), Univ Maryland Baltimore Cty, Goddard Earth Sci & Technol Ctr, Baltimore, MD 21228 USA. EM Thomas.W.Narock@nasa.gov OI Narock, Tom/0000-0002-9785-4496 FU NASA Research Opportunities in Space and Earth Sciences [NNX07AC95G] FX This work was supported under NASA Research Opportunities in Space and Earth Sciences grant NNX07AC95G. The authors would like to thank the SPASE consortium and Virtual Observatory members for helpful discussions during the development of this work. NR 7 TC 4 Z9 4 U1 0 U2 0 PU SPRINGER HEIDELBERG PI HEIDELBERG PA TIERGARTENSTRASSE 17, D-69121 HEIDELBERG, GERMANY SN 1865-0473 J9 EARTH SCI INFORM JI Earth Sci. Inform. PD APR PY 2008 VL 1 IS 1 BP 43 EP 48 DI 10.1007/s12145-008-0007-2 PG 6 WC Computer Science, Interdisciplinary Applications; Geosciences, Multidisciplinary SC Computer Science; Geology GA V15EM UT WOS:000207785300008 ER PT J AU Whitacre, JF Valdez, TI Narayanan, SR AF Whitacre, J. F. Valdez, T. I. Narayanan, S. R. TI A high-throughput study of PtNiZr catalysts for application in PEM fuel cells SO ELECTROCHIMICA ACTA LA English DT Article DE PEM fuel cell catalyst; PtNi; PtNiZr; combinatorial; thin film; sputter deposition ID OXYGEN REDUCTION REACTION; ALLOY ELECTRODES; ELECTROCATALYSTS; ELECTROREDUCTION; SURFACES; FE; NI; CO AB The effects of adding Zr to PtNi oxygen reduction reaction (ORR) electrocatalyst alloys were examined in a study aimed at probing the possibility of creating catalysts with enhanced resistance to corrosion in a PEM fuel cell environment. Samples consisting of pure Pt or PtNiZr alloys with a range of compositions (not exceeding 11 at.% Zr) were fabricated using co-sputter deposition. A high-throughput fabrication approach was used wherein 18 distinct thin film catalyst alloy samples with varying compositions were deposited onto a large-area substrate with individual Au current collector structures. A multi-channel pseudo-potentiostat allowed for the simultaneous quantitative study of catalytic activity for all 18 electrodes in a single test bath, a first for the study of ORR electrocatalysts. A properly stirred oxygenated I M H2SO4 electrolyte solution was used to provide each electrode with a steady-state flow of reactants during electrochemical evaluation. The onset potentials, absolute current density values, and Tafel analysis data obtained using this technique were compared with literature reports. The analyses showed that most PtNiZr alloys tested offered improvements over pure Pt, however those surfaces with a high mole fraction (>4 at.%) of Zr exhibited reduced activity that was roughly inversely correlated to the amount of Zr present. Film composition, morphology, and crystallographic properties were examined using X-ray energy dispersive spectroscopy (XEDS), X-ray photoelectron spectroscopy (XPS), SEM, and synchrotron X-ray diffraction. These data were then correlated with electrochemical data to elucidate the relationships between composition, structure, and relative performance for this ternary system. (c) 2007 Elsevier Ltd. All rights reserved. C1 [Whitacre, J. F.] Carnegie Mellon Univ, Dept Mat Sci & Engn, Pittsburgh, PA 15213 USA. [Whitacre, J. F.] Carnegie Mellon Univ, Dept Engn & Publ Policy, Pittsburgh, PA 15213 USA. [Valdez, T. I.; Narayanan, S. R.] CALTECH, Jet Prop Lab, Electrochem Technol Grp, Pasadena, CA 91109 USA. RP Whitacre, JF (reprint author), Carnegie Mellon Univ, Dept Mat Sci & Engn, 4323 Wean Hall, Pittsburgh, PA 15213 USA. EM whitacre@andrew.cinu.edu NR 20 TC 20 Z9 20 U1 3 U2 23 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0013-4686 J9 ELECTROCHIM ACTA JI Electrochim. Acta PD APR 1 PY 2008 VL 53 IS 10 BP 3680 EP 3689 DI 10.1016/j.electacta.2007.12.017 PG 10 WC Electrochemistry SC Electrochemistry GA 279KO UT WOS:000254354300015 ER PT J AU Menon, S Unger, N Koch, D Francis, J Garrett, T Sednev, I Shindell, D Streets, D AF Menon, Surabi Unger, Nadine Koch, Dorothy Francis, Jennifer Garrett, Tim Sednev, Igor Shindell, Drew Streets, David TI Aerosol climate effects and air quality impacts from 1980 to 2030 SO ENVIRONMENTAL RESEARCH LETTERS LA English DT Article DE aerosols; ozone; radiative forcing ID BLACK CARBON; EMISSIONS; CLOUDS; SENSITIVITY; SIMULATIONS; OZONE; INDIA; CHINA AB We investigate aerosol effects on climate for 1980, 1995 ( meant to reflect present day) and 2030 using the NASA Goddard Institute for Space Studies climate model coupled to an on-line aerosol source and transport model with interactive oxidant and aerosol chemistry. Aerosols simulated include sulfates, organic matter ( OM), black carbon ( BC), sea-salt and dust and, additionally, the amount of tropospheric ozone is calculated, allowing us to estimate both changes to air quality and climate for different time periods and emission amounts. We include both the direct aerosol effect and indirect aerosol effects for liquid-phase clouds. Future changes for the 2030 A1B scenario are examined, focusing on the Arctic and Asia, since changes are pronounced in these regions. Our results for the different time periods include both emission changes and physical climate changes. We find that the aerosol indirect effect ( AIE) has a large impact on photochemical processing, decreasing ozone amount and ozone forcing, especially for the future ( 2030-1995). Ozone forcings increase from 0 to 0.12 W m(-2) and the total aerosol forcing decreases from -0.10 to -0.94W m(-2) ( AIE decreases from -0.13 to -0.68W m(-2)) for 1995-1980 versus 2030-1995. Over the Arctic we find that compared to ozone and the direct aerosol effect, the AIE contributes the most to net radiative flux changes. The AIE, calculated for 1995-1980, is positive (1.0 W m(-2)), but the magnitude decreases (-0.3Wm(-2)) considerably for the future scenario. Over Asia, we evaluate the role of biofuel- and transportation- based emissions ( for BC and OM) via a scenario ( 2030A) that includes a projected increase ( factor of 2) in biofuel- and transport-based emissions for 2030 A1B over Asia. Projected changes from present day due to the 2030A emissions versus 2030 A1B are a factor of 4 decrease in summertime precipitation in Asia. Our results are sensitive to emissions used. Uncertainty in present-day emissions suggests that future climate projections warrant particular scrutiny. C1 [Menon, Surabi; Sednev, Igor] Univ Calif Berkeley, Lawrence Berkeley Lab, Berkeley, CA 94720 USA. [Unger, Nadine; Koch, Dorothy; Shindell, Drew] Columbia Univ, New York, NY USA. [Unger, Nadine; Koch, Dorothy; Shindell, Drew] NASA, Goddard Inst Space Studies, New York, NY 10025 USA. [Francis, Jennifer] Rutgers State Univ, New Brunswick, NJ 08903 USA. [Garrett, Tim] Univ Utah, Salt Lake City, UT USA. [Streets, David] Argonne Natl Lab, Argonne, IL 60439 USA. RP Menon, S (reprint author), Univ Calif Berkeley, Lawrence Berkeley Lab, Berkeley, CA 94720 USA. EM smenon@lbl.gov RI Shindell, Drew/D-4636-2012; Unger, Nadine/M-9360-2015; OI Streets, David/0000-0002-0223-1350 NR 38 TC 30 Z9 31 U1 1 U2 24 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 1748-9326 J9 ENVIRON RES LETT JI Environ. Res. Lett. PD APR-JUN PY 2008 VL 3 IS 2 AR 024004 DI 10.1088/1748-9326/3/2/024004 PG 12 WC Environmental Sciences; Meteorology & Atmospheric Sciences SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences GA 319PX UT WOS:000257177300005 ER PT J AU Hays, MD Beck, L Barfield, P Lavrich, RJ Dong, YJ Vander Wal, RL AF Hays, Michael D. Beck, Lee Barfield, Pamela Lavrich, Richard J. Dong, Yuanji Vander Wal, Randy L. TI Physical and chemical characterization of residential oil boiler emissions SO ENVIRONMENTAL SCIENCE & TECHNOLOGY LA English DT Article ID FINE-PARTICLE EMISSIONS; ULTRAFINE PARTICLES; FUEL-OIL; SIZE DISTRIBUTIONS; AEROSOL EMISSIONS; COMBUSTION; SAMPLER; MATTER; MASS AB The toxicity of emissions from the combustion of home heating oil coupled with the regional proximity and seasonal use of residential oil boilers (ROB) is an important public health concern. Yet scant physical and chemical information about the emissions from this source is available for climate and air quality modeling and for improving our understanding of aerosol-related human health effects. The gas- and particle-phase emissions from an active ROB firing distillate fuel oil (commonly known as diesel fuel) were evaluated to address this deficiency. Ion chromatography of impactor samples showed that the ultrafine ROB aerosol emissions were similar to 45% (w/w) sulfate. Gas chromatography-mass spectrometry detected various n-alkanes at trace levels, sometimes in accumulation mode particles, and out of phase with the size distributions of aerosol mass and sulfate. The carbonaceous matter in the ROB aerosol was primarily light-adsorbing elemental carbon. Gas chromatography-atomic emission spectroscopy measured a previously unrecognized organosulfur compound group in the ROB aerosol emissions. High-resolution transmission electron microscopy of ROB soot indicated the presence of a highly ordered primary particle nanostructure embedded in larger aggregates. Organic gas emissions were measured using EPA Methods TO-15 and TO-11A. The ROB emitted volatile oxygenates (8 mg/(kg of oil burned)) and olefins (5 mg/(kg of oil burned)) mostly unrelated to the base fuel composition. In the final analysis, the ROB tested was a source of numerous hazardous air pollutants as defined in the Clean Air Act Amendments. Approximations conducted using emissions data from the ROB tests show relatively low contributions to a regional-level anthropogenic emissions inventory for volitile organic compounds, PM2.5, and SO2 mass. C1 [Hays, Michael D.; Beck, Lee; Barfield, Pamela; Lavrich, Richard J.] US EPA, Natl Risk Management Res Lab, Res Triangle Pk, NC 27711 USA. [Dong, Yuanji] ARCADIS, Res Triangle Pk, NC 27711 USA. [Vander Wal, Randy L.] NASA, Glenn Res Ctr, Univ Space Res Assoc, Cleveland, OH 44135 USA. RP Hays, MD (reprint author), US EPA, Natl Risk Management Res Lab, Res Triangle Pk, NC 27711 USA. EM hays.michael@epa.gov RI Hays, Michael/E-6801-2013; Wang, Linden/M-6617-2014 OI Hays, Michael/0000-0002-4029-8660; NR 38 TC 13 Z9 13 U1 3 U2 29 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 0013-936X EI 1520-5851 J9 ENVIRON SCI TECHNOL JI Environ. Sci. Technol. PD APR 1 PY 2008 VL 42 IS 7 BP 2496 EP 2502 DI 10.1021/es071598e PG 7 WC Engineering, Environmental; Environmental Sciences SC Engineering; Environmental Sciences & Ecology GA 281JN UT WOS:000254492800047 PM 18504987 ER PT J AU Gustafsson, T Osterlund, T von Walden, F Trappe, T Linnehan, R Tesch, P AF Gustafsson, Thomas Osterlund, Ted von Walden, Ferdinand Trappe, Todd Linnehan, Rick Tesch, Per TI Three days of unloading induces pre-translational changes in human skeletal muscle SO FASEB JOURNAL LA English DT Meeting Abstract C1 [Gustafsson, Thomas; Osterlund, Ted; von Walden, Ferdinand; Tesch, Per] Karolinska Inst, Stockholm, Sweden. [Osterlund, Ted; Tesch, Per] Mid Univ, Ostersund, Sweden. [Trappe, Todd] Ball State Univ, Muncie, IN 47306 USA. [Linnehan, Rick] NASA, Houston, TX USA. NR 0 TC 0 Z9 0 U1 0 U2 1 PU FEDERATION AMER SOC EXP BIOL PI BETHESDA PA 9650 ROCKVILLE PIKE, BETHESDA, MD 20814-3998 USA SN 0892-6638 J9 FASEB J JI Faseb J. PD APR PY 2008 VL 22 PG 1 WC Biochemistry & Molecular Biology; Biology; Cell Biology SC Biochemistry & Molecular Biology; Life Sciences & Biomedicine - Other Topics; Cell Biology GA V25GZ UT WOS:000208467807289 ER PT J AU Hitchcox, K Wolf, M Zwart, SR Smith, SM AF Hitchcox, Kristen Wolf, Megan Zwart, Sara R. Smith, Scott M. TI Stability of biochemical analytes in blood specimens subjected to delayed processing SO FASEB JOURNAL LA English DT Meeting Abstract C1 [Hitchcox, Kristen] Colby Coll, Waterville, ME 04901 USA. [Zwart, Sara R.] Univ Space Res Assoc, Houston, TX USA. [Smith, Scott M.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. NR 0 TC 0 Z9 0 U1 1 U2 1 PU FEDERATION AMER SOC EXP BIOL PI BETHESDA PA 9650 ROCKVILLE PIKE, BETHESDA, MD 20814-3998 USA SN 0892-6638 J9 FASEB J JI Faseb J. PD APR PY 2008 VL 22 PG 1 WC Biochemistry & Molecular Biology; Biology; Cell Biology SC Biochemistry & Molecular Biology; Life Sciences & Biomedicine - Other Topics; Cell Biology GA V25GZ UT WOS:000208467806518 ER PT J AU Howarth, MS Moore, FB Hinghofer-Szalkay, H Jezova, D Diedrich, A Ferris, M Schlegel, TT Patwardhan, AR Knapp, CF Evans, JM AF Howarth, Mark S. Moore, Fritz B. Hinghofer-Szalkay, Helmut Jezova, Daniela Diedrich, Andre' Ferris, Mead Schlegel, Todd T. Patwardhan, Abhijit R. Knapp, Charles F. Evans, Joyce M. TI Thoracic impedance as a potential indicator of Gz-induced presyncope SO FASEB JOURNAL LA English DT Meeting Abstract C1 [Howarth, Mark S.; Ferris, Mead; Patwardhan, Abhijit R.; Knapp, Charles F.; Evans, Joyce M.] Univ Kentucky, Ctr Biomed Engn, Lexington, KY 40506 USA. [Moore, Fritz B.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Hinghofer-Szalkay, Helmut] Inst Adapt & Spaceflight Physiol, Graz, Austria. [Jezova, Daniela] Inst Expt Endocrinol SAS, Bratislava, Slovakia. [Diedrich, Andre'] Vanderbilt Univ, Auton Dysfunct Ctr, Nashville, TN USA. [Schlegel, Todd T.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. NR 0 TC 0 Z9 0 U1 0 U2 1 PU FEDERATION AMER SOC EXP BIOL PI BETHESDA PA 9650 ROCKVILLE PIKE, BETHESDA, MD 20814-3998 USA SN 0892-6638 J9 FASEB J JI Faseb J. PD APR PY 2008 VL 22 PG 1 WC Biochemistry & Molecular Biology; Biology; Cell Biology SC Biochemistry & Molecular Biology; Life Sciences & Biomedicine - Other Topics; Cell Biology GA V25GZ UT WOS:000208467807204 ER PT J AU Liang, MTC Lewis, KM Spalding, TW Bassin, SL Arnaud, SB AF Liang, Michael T. C. Lewis, Kevin M. Spalding, Thomas W. Bassin, Stan L. Arnaud, Sara B. TI Bone Bending Stiffness and BMD in trained Cyclists, Runners and Untrained Men SO FASEB JOURNAL LA English DT Meeting Abstract C1 [Liang, Michael T. C.; Lewis, Kevin M.; Spalding, Thomas W.] Calif State Polytech Univ Pomona, Pomona, CA 91768 USA. [Bassin, Stan L.] UCI Med Ctr, Inst Clin & Translat Sci, Irvine, CA USA. [Arnaud, Sara B.] NASA AMES, Life Sci Div, Moffett Field, CA USA. NR 0 TC 0 Z9 0 U1 0 U2 2 PU FEDERATION AMER SOC EXP BIOL PI BETHESDA PA 9650 ROCKVILLE PIKE, BETHESDA, MD 20814-3998 USA SN 0892-6638 J9 FASEB J JI Faseb J. PD APR PY 2008 VL 22 PG 1 WC Biochemistry & Molecular Biology; Biology; Cell Biology SC Biochemistry & Molecular Biology; Life Sciences & Biomedicine - Other Topics; Cell Biology GA V25GY UT WOS:000208467700703 ER PT J AU Macias, BR Schneider, S Lee, SMC Guinet, P Hughson, R Smith, S Watenpaugh, D Hargens, A AF Macias, Brandon Richard Schneider, Suzanne Lee, Stuart M. C. Guinet, Patrick Hughson, Richard Smith, Scott Watenpaugh, Donald Hargens, Alan TI WISE-2005: Lower Body Negative Pressure Treadmill and Resistive Exercise Countermeasures Maintain Physiologic Function in Women during 60-days of Simulated Microgravity SO FASEB JOURNAL LA English DT Meeting Abstract C1 [Macias, Brandon Richard; Guinet, Patrick; Watenpaugh, Donald; Hargens, Alan] Univ Calif San Diego, San Diego, CA 92103 USA. [Schneider, Suzanne] Univ New Mexico, Albuquerque, NM 87131 USA. [Lee, Stuart M. C.] Wyle Labs, Houston, TX USA. [Hughson, Richard] Univ Waterloo, Waterloo, ON N2L 3G1, Canada. [Smith, Scott] NASA, Houston, TX USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU FEDERATION AMER SOC EXP BIOL PI BETHESDA PA 9650 ROCKVILLE PIKE, BETHESDA, MD 20814-3998 USA SN 0892-6638 J9 FASEB J JI Faseb J. PD APR PY 2008 VL 22 PG 1 WC Biochemistry & Molecular Biology; Biology; Cell Biology SC Biochemistry & Molecular Biology; Life Sciences & Biomedicine - Other Topics; Cell Biology GA V25GZ UT WOS:000208467809411 ER PT J AU Meng, M Stenger, M Platts, S Feiveson, A Natapoff, A Knapp, C Evans, J Paloski, W AF Meng, Martha Stenger, Michael Platts, Steven Feiveson, Al Natapoff, Alan Knapp, Charles Evans, Joyce Paloski, William TI Cardiovascular mechanisms are maintained by intermittent artificial gravity exposure during bed rest deconditioning SO FASEB JOURNAL LA English DT Meeting Abstract C1 [Meng, Martha; Knapp, Charles; Evans, Joyce] Univ Kentucky, Ctr Biomed Engn, Lexington, KY 40506 USA. [Stenger, Michael] Wyle Labs, Houston, TX USA. [Platts, Steven; Feiveson, Al; Paloski, William] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. [Natapoff, Alan] MIT, Cambridge, MA 02139 USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU FEDERATION AMER SOC EXP BIOL PI BETHESDA PA 9650 ROCKVILLE PIKE, BETHESDA, MD 20814-3998 USA SN 0892-6638 J9 FASEB J JI Faseb J. PD APR PY 2008 VL 22 PG 1 WC Biochemistry & Molecular Biology; Biology; Cell Biology SC Biochemistry & Molecular Biology; Life Sciences & Biomedicine - Other Topics; Cell Biology GA V25GZ UT WOS:000208467806568 ER PT J AU Smith, SM Gardner, K Locke, J Zwart, SR AF Smith, Scott M. Gardner, Keri Locke, James Zwart, Sara R. TI Efficacy of vitamin D supplementation in an Antarctic ground analog of space flight SO FASEB JOURNAL LA English DT Meeting Abstract C1 [Smith, Scott M.; Locke, James] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. [Gardner, Keri] Univ Calif Los Angeles, Los Angeles, CA USA. [Zwart, Sara R.] Univ Space Res Assoc, Houston, TX USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU FEDERATION AMER SOC EXP BIOL PI BETHESDA PA 9650 ROCKVILLE PIKE, BETHESDA, MD 20814-3998 USA SN 0892-6638 J9 FASEB J JI Faseb J. PD APR PY 2008 VL 22 PG 1 WC Biochemistry & Molecular Biology; Biology; Cell Biology SC Biochemistry & Molecular Biology; Life Sciences & Biomedicine - Other Topics; Cell Biology GA V25GZ UT WOS:000208467808715 ER PT J AU Zwart, SR Smith, SM AF Zwart, Sara R. Smith, Scott M. TI Oxidative Damage during a 10-to 12-d Saturation Dive SO FASEB JOURNAL LA English DT Meeting Abstract C1 [Zwart, Sara R.] Univ Space Res Assoc, Houston, TX USA. [Smith, Scott M.] NASA Johnson Space Ctr, Houston, TX USA. NR 0 TC 0 Z9 0 U1 0 U2 1 PU FEDERATION AMER SOC EXP BIOL PI BETHESDA PA 9650 ROCKVILLE PIKE, BETHESDA, MD 20814-3998 USA SN 0892-6638 J9 FASEB J JI Faseb J. PD APR PY 2008 VL 22 PG 1 WC Biochemistry & Molecular Biology; Biology; Cell Biology SC Biochemistry & Molecular Biology; Life Sciences & Biomedicine - Other Topics; Cell Biology GA V25GZ UT WOS:000208467808689 ER PT J AU Orr, JW Hawkins, S AF Orr, James W. Hawkins, Sharon TI Species of the rougheye rockfish complex: resurrection of Sebastes melanostictus (Matsubara, 1934) and a redescription of Sebastes aleutianus (Jordan and Evermann, 1898) (Teleostei : Scorpaeniformes) SO FISHERY BULLETIN LA English DT Article ID NORTH PACIFIC-OCEAN; SYSTEMATICS AB The widespread and commercially important rougheye rockfish, Sebastes aleutianus (Jordan and Evermann, 1898), has been considered a single variable species, with light- and dark-colored forms, found on the outer continental shelf and upper slope of the North Pacific Ocean. Genetic analysis of 124 specimens verified the presence of two species in new specimens collected from Alaska to Oregon, and the two species were analyzed for distinguishing color patterns and morphological characters. Characters distinguishing the two were extended to an analysis of 215 additional formalin-fixed specimens representing their geographic ranges. Sebastes aleutianus is pale, often has dark mottling on the dorsum in diffuse bands, and does not have distinct dark spots on the spinous dorsal fin; it ranges from the eastern Aleutian Islands and southeastern Bering Sea to California. Sebastes melanostictus (Matsubara, 1934), the blackspotted rockfish, ranges from central Japan, through the Aleutian Islands and Bering Sea, to southern California. It is darker overall and spotting is nearly always present on the spinous dorsal fin. Sebastes swifti (Evermann and Goldsborough, 1907) is a synonym of S. aleutianus; S. kawaradae (Matsubara, 1934) is a synonym of S. melanostictus. The subgenus Zalopyr is restricted to S. aleutianus and S. melanostictus. Nomenclatural synonymies, diagnoses, descriptions, and distributions are provided for each species. C1 [Orr, James W.] NOAA, Natl Marine Fisheries Serv, Resource Assessment & Conservat Engn Div, Alaska Fisheries Sci Ctr, Seattle, WA 98115 USA. [Hawkins, Sharon] NOAA, Ted Stevens Marine Res Inst, Natl Marine Fisheries Serv, Alaska Fisheries Sci Ctr,Auke Bay Labs, Juneau, AK 99801 USA. RP Orr, JW (reprint author), NOAA, Natl Marine Fisheries Serv, Resource Assessment & Conservat Engn Div, Alaska Fisheries Sci Ctr, 7600 Sand Point Way NE, Seattle, WA 98115 USA. EM James.Orr@noaa.gov NR 60 TC 14 Z9 19 U1 0 U2 2 PU NATL MARINE FISHERIES SERVICE SCIENTIFIC PUBL OFFICE PI SEATTLE PA 7600 SAND POINT WAY NE BIN C15700, SEATTLE, WA 98115 USA SN 0090-0656 J9 FISH B-NOAA JI Fish. Bull. PD APR PY 2008 VL 106 IS 2 BP 111 EP 134 PG 24 WC Fisheries SC Fisheries GA 299CQ UT WOS:000255733800001 ER PT J AU Parnel, MM Emmett, RL Brodeur, RD AF Parnel, Maria M. Emmett, Robert L. Brodeur, Richard D. TI Ichthyoplankton community in the Columbia River plume off Oregon: effects of fluctuating oceanographic conditions SO FISHERY BULLETIN LA English DT Article ID CALIFORNIA CURRENT; NORTHEAST PACIFIC; JUVENILE SALMONIDS; FISH PRODUCTION; ABUNDANCE; CLIMATE; LARVAL; OCEAN; ZONE; RECRUITMENT AB Ichthyoplankton samples were collected at approximately 2-week intervals, primarily during spring and summer 1999-2004, from two stations located 20 and 30 km from shore near the Columbia River, Oregon. Northern anchovy (Engraulis mordax) was the most abundant species collected, and was the primary species associated with summer upwelling conditions, but it showed significant interannual and seasonal fluctuations in abundance and occurrence. Other abundant taxa included sanddabs (Citharichthys spp.), English sole (Parophrys vetulus), and blaeksmelts (Bathylagidae). Two-way cluster analysis revealed strong species associations based primarily on season (before or after the spring transition date). Ichthyoplankton abundances were compared to biological and environmental data, and egg and larvae abundances were found to be most correlated with sea surface temperature. The Pacific Decadal Oscillation changed sign (from negative to positive) in late 2002 and indicated overall warmer conditions in the North Pacific Ocean. Climate change is expected to alter ocean upwelling, temperatures, and Columbia River flows, and consequently fish eggs and larvae distributions and survival. Long-term research is needed to identify how ichthyoplankton and fish recruitment are affected by regional and large-scale oceanographic processes. C1 [Parnel, Maria M.; Emmett, Robert L.; Brodeur, Richard D.] Hatfield Marine Sci Ctr, Natl Marine Fisheries Serv, Natl Ocean & Atmospher Adm, Newport, OR USA. RP Parnel, MM (reprint author), Hatfield Marine Sci Ctr, Natl Marine Fisheries Serv, Natl Ocean & Atmospher Adm, 2030 S Marine Sci Dr, Newport, OR USA. EM Robert.Emmett@noaa.gov NR 62 TC 20 Z9 20 U1 3 U2 9 PU NATL MARINE FISHERIES SERVICE SCIENTIFIC PUBL OFFICE PI SEATTLE PA 7600 SAND POINT WAY NE BIN C15700, SEATTLE, WA 98115 USA SN 0090-0656 J9 FISH B-NOAA JI Fish. Bull. PD APR PY 2008 VL 106 IS 2 BP 161 EP 173 PG 13 WC Fisheries SC Fisheries GA 299CQ UT WOS:000255733800005 ER PT J AU McKean, JA Isaak, DJ Wright, CW AF McKean, Jim A. Isaak, Dan J. Wright, Charles W. TI Geomorphic controls on salmon nesting patterns described by a new, narrow-beam terrestrial-aquatic lidar SO FRONTIERS IN ECOLOGY AND THE ENVIRONMENT LA English DT Article ID LANDSCAPES AB Riverine aquatic biodiversity is rapidly being lost worldwide, but preservation efforts are hampered, in part because studies of these dynamic environments are limited by cost and logistics to small local surveys. Full understanding of stream ecosystems requires precise, high-resolution mapping of entire stream networks and adjacent landforms. We use a narrow-beam, water-penetrating, green lidar system to continuously map 10 km of a mountain stream channel, including its floodplain topography, and wavelet analyses to investigate spatial patterns of channel morphology and salmon spawning. Results suggest the broadest fluvial domains are a legacy of approximately 15 000 years of post-glacial valley evolution and that local pool-riffle channel topography is controlled by contemporary hydraulics operating on this broad template. Salmon spawning patterns closely reflect these hierarchical physical domains, demonstrating how geomorphic history can influence modem distributions of aquatic habitat and organisms. The new terrestrial-aquatic lidar could catalyze rapid advances in understanding, managing, and monitoring of valuable aquatic ecosystems through unprecedented and attendant analyses. C1 [McKean, Jim A.; Isaak, Dan J.] US Forest Serv, Rocky Mt Res Stn, Boise, ID 83702 USA. [Wright, Charles W.] NASA, Goddard Space Flight Ctr, Wallops Flight Facil, Wallops Isl, VA 23337 USA. RP McKean, JA (reprint author), US Forest Serv, Rocky Mt Res Stn, Boise, ID 83702 USA. EM jmckean@fs-fed.us RI McKean, Jim/C-3581-2011; Isaak, Dan/C-8818-2011 NR 16 TC 46 Z9 47 U1 3 U2 12 PU ECOLOGICAL SOC AMER PI WASHINGTON PA 1707 H ST NW, STE 400, WASHINGTON, DC 20006-3915 USA SN 1540-9295 J9 FRONT ECOL ENVIRON JI Front. Ecol. Environ. PD APR PY 2008 VL 6 IS 3 BP 125 EP 130 DI 10.1890/070109 PG 6 WC Ecology; Environmental Sciences SC Environmental Sciences & Ecology GA 282WF UT WOS:000254597200017 ER PT J AU Asgharzadeh, MF von Frese, RRB Kim, HR AF Asgharzadeh, M. F. von Frese, R. R. B. Kim, H. R. TI Spherical prism magnetic effects by Gauss-Legendre quadrature integration SO GEOPHYSICAL JOURNAL INTERNATIONAL LA English DT Article DE magnetic anomalies : modelling and interpretation; satellite magnetics; planetary tectonics ID EARTH GRAVITY; ANOMALY MAP; SATELLITE; INVERSION AB Regional spherical coordinate observations of the Earth's crustal magnetic field components are becoming increasingly available from shipborne, airborne, and satellite surveys. In assessing the geological significance of these data, theoretical anomalous magnetic fields from geologic models in spherical coordinates need to be evaluated. This study explicitly develops the elegant Gauss-Legendre quadrature formulation for numerically modelling the complete magnetic effects (i.e. potential, vector and tensor gradient fields) of the spherical prism. We also use these results to demonstrate the magnetic effects for the crustal prism and to investigate the crustal magnetic effects at satellite altitudes for a large region of the Middle East centred on Iran. C1 [Asgharzadeh, M. F.; von Frese, R. R. B.] Ohio State Univ, Sch Earth Sci, Columbus, OH 43210 USA. [Kim, H. R.] Univ Maryland Baltimore Cty, Goddard Earth Sci & Technol Ctr, GSFC NASA, Greenbelt, MD 20771 USA. RP Asgharzadeh, MF (reprint author), Ohio State Univ, Sch Earth Sci, Columbus, OH 43210 USA. EM vonfrese@osu.edu NR 33 TC 5 Z9 6 U1 1 U2 3 PU BLACKWELL PUBLISHING PI OXFORD PA 9600 GARSINGTON RD, OXFORD OX4 2DQ, OXON, ENGLAND SN 0956-540X J9 GEOPHYS J INT JI Geophys. J. Int. PD APR PY 2008 VL 173 IS 1 BP 315 EP 333 DI 10.1111/j.1365-246X.2007.03692.x PG 19 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 276FJ UT WOS:000254126400022 ER PT J AU Trout, TJ Johnson, LF Gartung, J AF Trout, Thomas J. Johnson, Lee F. Gartung, Jim TI Remote sensing of canopy cover in horticultural crops SO HORTSCIENCE LA English DT Article; Proceedings Paper CT Annual Conference of the American-Society-for-Horticultural-Science CY JUL 25-30, 2006 CL New Orleans, LA SP Amer Soc Horticultural Sci DE evapotranspiration; shaded area; NDVI; vegetation index; fractional cover; crop coefficients ID SHADED AREA; COEFFICIENTS; VEGETATION; RADIATION; INDEX; CORN AB Canopy cover (CC) is an important indicator of stage of growth and crop water use in horticultural crops. Remote sensing of CC has been studied in several major crops, but not in most horticultural crops. We measured CC of 11 different annual and perennial horticultural crops in various growth stages on 30 fields on the west side of California's San Joaquin Valley with a handheld multispectral digital camera. Canopy cover was compared with normalized difference vegetation index (NDVI) values calculated from Landsat 5 satellite imagery. The NDVI was highly correlated and linearly related with measured CC across the wide range of crops, canopy structures, and growth stages (R-2 = 0.95, P < 0.01) and predicted CC with mean absolute error of 0.047 up to effective full cover. These results indicate that remotely sensed NDVI may be an efficient way to monitor growth stage, and potentially irrigation water demand, of horticultural crops. C1 [Trout, Thomas J.] USDA ARS, Ft Collins, CO 80526 USA. [Johnson, Lee F.] NASA, Ames Res Ctr, CSUMB SEP, Div Earth Sci, Moffett Field, CA 94035 USA. [Gartung, Jim] USDA ARS, Parlier, CA 93548 USA. RP Trout, TJ (reprint author), USDA ARS, 2150 Ctr Dr,Bldg D, Ft Collins, CO 80526 USA. EM Thomas.Trout@ars.usda.gov OI Trout, Thomas/0000-0003-1896-9170 NR 22 TC 24 Z9 24 U1 0 U2 11 PU AMER SOC HORTICULTURAL SCIENCE PI ALEXANDRIA PA 113 S WEST ST, STE 200, ALEXANDRIA, VA 22314-2851 USA SN 0018-5345 EI 2327-9834 J9 HORTSCIENCE JI Hortscience PD APR PY 2008 VL 43 IS 2 BP 333 EP 337 PG 5 WC Horticulture SC Agriculture GA 274UC UT WOS:000254026400012 ER PT J AU Mitchell, DL Halekas, JS Lin, RP Frey, S Hood, LL Acuna, MH Binder, A AF Mitchell, D. L. Halekas, J. S. Lin, R. P. Frey, S. Hood, L. L. Acuna, M. H. Binder, A. TI Global mapping of lunar crustal magnetic fields by Lunar Prospector SO ICARUS LA English DT Article DE Moon; surface; magnetic fields; cratering; impact processes ID IMPACT BASINS; RIMA-SIRSALIS; ANOMALIES; SURFACE; MODEL; MARS AB The Lunar Prospector Electron Reflectometer has obtained the first global map of lunar crustal magnetic fields, revealing that the effects of basin-forming impacts dominate the large-scale distribution of remanent magnetic fields on the Moon. The weakest surface magnetic fields (<0.2 nT) are found within two of the largest and most recent impact basins, Orientale and Imbrium. Conversely, the largest concentrations of strong surface fields (>40 nT) are diametrically opposite to these same basins. This pattern is present though less pronounced for several other post-Nectarian impact basins larger than 500 km in diameter. The reduced strength and clarity of the pattern for older basins may be attributed to: (1) demagnetization from many smaller impacts, which erases antipodal magnetic signatures over time, (2) superposition effects from other large impacts, and (3) variation in the strength of the ambient magnetizing field. The absence of fringing fields stronger than I nT around the perimeter of the Imbrium basin or associated with craters within the basin implies that any uniform magnetization of the impact melt must be weaker than similar to 10(-6) G cm(3) g(-1). This limits the strength of any steady ambient magnetic field to no more than similar to 0.1 Oe at the lunar surface while the basin cooled for tens of millions of years following the Imbrium impact 3.8 billion years ago. (C) 2008 Elsevier Inc. All rights reserved. C1 [Mitchell, D. L.; Halekas, J. S.; Lin, R. P.; Frey, S.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Lin, R. P.] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA. [Hood, L. L.] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA. [Acuna, M. H.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Binder, A.] Lunar Res Inst, Tucson, AZ 85747 USA. RP Mitchell, DL (reprint author), Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. EM mitchell@ssl.berkeley.edu OI Halekas, Jasper/0000-0001-5258-6128 NR 40 TC 79 Z9 83 U1 1 U2 7 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 J9 ICARUS JI Icarus PD APR PY 2008 VL 194 IS 2 BP 401 EP 409 DI 10.1016/j.icarus.2007.10.027 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 284DM UT WOS:000254685900002 ER PT J AU Malin, MC Calvin, WM Cantor, BA Clancy, RT Haberle, RM James, PB Thomas, PC Wolff, MJ Bell, JE Lee, SW AF Malin, Michael C. Calvin, Wendy M. Cantor, Bruce A. Clancy, R. Todd Haberle, Robert M. James, Philip B. Thomas, Peter C. Wolff, Michael J. Bell, James E., III Lee, Steven W. TI Climate, weather, and north polar observations from the Mars Reconnaissance Orbiter Mars Color Imager SO ICARUS LA English DT Article DE Mars, atmosphere; Mars, polar caps ID HUBBLE-SPACE-TELESCOPE; LASER ALTIMETER; WATER ICE; CLOUDS; APHELION; VIKING; SIMULATION; ATMOSPHERE; BEHAVIOR; AEROSOL AB The Mars Reconnaissance Orbiter observes Mars from a nearly circular, polar orbit. From this vantage point, the Mars Color Imager extends the similar to 5 Mars years record of Mars Global Surveyor global, visible-wavelength multi-color observations of meteorological events and adds measurements at three additional visible and two ultraviolet wavelengths. Observations of the global distribution of ozone (which anti-correlates with water vapor) and water ice and dust clouds allow tracking of atmospheric circulation. Regional and local observations emphasize smaller scale atmospheric dynamics, especially those related to dust lifting and subsequent motion. Polar observations detail variations related to the polar heat budget, including changes in polar frosts and ices, and storms generated at high thermal contrast boundaries. (C) 2007 Elsevier Inc. All rights reserved. C1 [James, Philip B.; Thomas, Peter C.] Cornell Univ, Ctr Radiophys & Space Res, Ithaca, NY 14853 USA. [Malin, Michael C.; Cantor, Bruce A.] Malin Space Syst, San Diego, CA 92191 USA. [Bell, James E., III] Cornell Univ, Dept Astron, Ithaca, NY 14853 USA. [Calvin, Wendy M.] Univ Nevada, Dept Geol Sci, Reno, NV 89557 USA. [Clancy, R. Todd; Wolff, Michael J.; Lee, Steven W.] Space Sci Inst, Boulder, CO 80301 USA. [Haberle, Robert M.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Lee, Steven W.] Denver Museum Nat & Sci, Denver, CO 80205 USA. RP James, PB (reprint author), Cornell Univ, Ctr Radiophys & Space Res, Ithaca, NY 14853 USA. EM pjames@cableone.net NR 37 TC 21 Z9 21 U1 1 U2 9 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 J9 ICARUS JI Icarus PD APR PY 2008 VL 194 IS 2 BP 501 EP 512 DI 10.1016/j.icarus.2007.10.016 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 284DM UT WOS:000254685900009 ER PT J AU Barr, AC Milkovich, SM AF Barr, Amy C. Milkovich, Sarah M. TI Ice grain size and the rheology of the martian polar deposits SO ICARUS LA English DT Article DE Mars; ices ID DYNAMIC RECRYSTALLIZATION; MARS; CAP; STRESS; FLOW; TEMPERATURE; DEPENDENCE; GREENLAND; TEXTURES; FABRICS AB The history and dynamics of the martian polar deposits (MPD), the largest known water reservoirs on Mars, are of great interest, but estimates of ice grain size are required before detailed modeling can be performed. We clarify the microphysical processes that may control grain size in the MPD. If the MPD are similar to 2% dust by mass, the maximum ice grain size is similar to 1 mm due to grain boundary pinning by silicate microparticles. Relatively dusty layers in the MPD will have smaller grain sizes. If MPD ice has a very low impurity content and has experienced a significant amount of strain, grains may reach a steady state size of similar to 1.5 to 3 mm due to dynamic recrystallization, wherein a steady state grain size is maintained due to the balance of grain growth and destruction during flow. If the near-bed ice in the MPD is warmed close to its melting point and has been extensively sheared, grain sizes at its base may be between 10 and 40 mm, by analogy with warm, dirty, near-bed ice in terrestrial ice sheets. (C) 2007 Elsevier Inc. All rights reserved. C1 [Barr, Amy C.] SW Res Inst, Dept Space Studies, Boulder, CO 80302 USA. [Milkovich, Sarah M.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Barr, AC (reprint author), SW Res Inst, Dept Space Studies, 1050 Walnut St,Suite 300, Boulder, CO 80302 USA. EM amy@boulder.swri.edu NR 32 TC 10 Z9 10 U1 0 U2 2 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 J9 ICARUS JI Icarus PD APR PY 2008 VL 194 IS 2 BP 513 EP 518 DI 10.1016/j.icarus.2007.11.018 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 284DM UT WOS:000254685900010 ER PT J AU Lillis, RJ Mitchell, DL Lin, RP Acuna, MH AF Lillis, Robert J. Mitchell, David L. Lin, Robert P. Acuna, Mario H. TI Electron reflectometry in the martian atmosphere SO ICARUS LA English DT Article DE Mars; magnetic fields; Mars, atmosphere ID SPHERICAL HARMONIC MODEL; CRUSTAL MAGNETIC-FIELD; SOLAR-CYCLE VARIATION; MARS GLOBAL SURVEYOR; IMPACT IONIZATION; LUNAR PROSPECTOR; CROSS-SECTIONS; ARGON; IONOSPHERE; EXCITATION AB The technique of electron reflectometry, a method for remote estimation of planetary magnetic fields, is expanded from its original use of mapping crustal magnetic fields at the Moon to achieving the same purpose at Mars, where the presence of a substantial atmosphere complicates matters considerably. The motion of solar wind electrons, incident on the martian atmosphere, is considered in detail, taking account of the following effects: the electrons' helical paths around the magnetic field lines to which they are bound, the magnetic mirror force they experience due to converging field lines in the vicinity of crustal magnetic anomalies, their acceleration/deceleration by electrostatic potentials, their interactions with thermal plasma. their drifts due to magnetic field line curvature and perpendicular electric fields and their scattering off, and loss of energy through a number of different processes to, atmospheric neutrals. A theoretical framework is thus developed for modeling electron pitch angle distributions expected when a spacecraft is on a magnetic field line which is connected to both the martian crust and the interplanetary magnetic field. This framework, along with measured pitch angle distributions from the Mars Global Surveyor (MGS) Magnetometer/Electron Reflectometer (MAG/ER) experiment, can be used to remotely measure crustal magnetic field magnitudes and atmospheric neutral densities at similar to 180 km above the martian datum, as well as estimate average parallel electric fields between 200 and 400 km altitude. Detailed analysis and full results, concerning the crustal magnetic field and upper thermospheric density of Mars, are left to two companion papers. (C) 2007 Elsevier Inc. All rights reserved. C1 [Lillis, Robert J.; Mitchell, David L.; Lin, Robert P.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Acuna, Mario H.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Lillis, RJ (reprint author), Univ Calif Berkeley, Space Sci Lab, 7 Gauss Way, Berkeley, CA 94720 USA. EM rlillis@ssl.berkeley.edu RI Lillis, Robert/A-3281-2008 OI Lillis, Robert/0000-0003-0578-517X NR 56 TC 22 Z9 22 U1 0 U2 4 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 J9 ICARUS JI Icarus PD APR PY 2008 VL 194 IS 2 BP 544 EP 561 DI 10.1016/j.icarus.2007.09.030 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 284DM UT WOS:000254685900012 ER PT J AU Lillis, RJ Bougher, SW Mitchell, DL Brain, DA Lin, RP Acuna, MH AF Lillis, Robert J. Bougher, Stephen W. Mitchell, David L. Brain, David A. Lin, Robert P. Acuna, Mario H. TI Continuous monitoring of nightside upper thermospheric mass densities in the martian southern hemisphere over 4 martian years using electron reflectometry SO ICARUS LA English DT Article DE Mars; magnetic fields; Mars, atmosphere ID GENERAL-CIRCULATION MODEL; SPHERICAL HARMONIC MODEL; CRUSTAL MAGNETIC-FIELD; SOLAR-CYCLE VARIATION; MARS GLOBAL SURVEYOR; UPPER-ATMOSPHERE; MGS ACCELEROMETER; HIGH-ALTITUDE; SIMULATIONS; IONOSPHERE AB Details are presented of an improved technique to use atmospheric absorption of magnetically reflecting solar wind electrons to constrain neutral mass densities in the nightside martian upper thermosphere. The helical motion of electrons on converging magnetic field lines, through an extended neutral atmosphere, is modeled to enable prediction of loss cone pitch angle distributions measured by the Magnetometer/Electron Reflectometer (MAG/ER) experiment on Mars Global Surveyor at 400 km altitude. Over the small fraction of Mars' southern hemisphere (similar to 2.5%) where the permanent crustal magnetic fields are both open to the solar wind and sufficiently strong as to dominate the variable induced martian magnetotail field, spherical harmonic expansions of the crustal fields are used to prescribe the magnetic field along the electron's path, allowing least-squares fitting of measured loss cones, in order to solve for parameters describing the vertical neutral atmospheric mass density profile from 160 to 230 km. Results are presented of mass densities in the southern hemisphere at 2 a.m. LST at the mean altitude of greatest sensitivity, 180 km. continuously over four martian years. Seasonal variability in densities is largely explained by orbital and latitudinal changes in dayside insolation that impacts the nightside through the resulting thermospheric circulation. However, the physical processes behind repeatable rapid, late autumnal cooling at mid-latitudes and near-aphelion warming at equatorial latitudes is not fully clear. Southern winter polar warming is generally weak or nonexistent over several Mars years, in basic agreement with MGS and MRO accelerometer observations. The puzzling response of mid-latitude densities from 160 degrees to 200 degrees E to the 2001 global dust storm suggests unanticipated localized nightside upper thermospheric lateral and vertical circulation patterns may accompany such storms. The downturn of the 11-year cycle of solar EUV flux is likely responsible for lower aphelion densities in 2004 and 2006 (Mars years 27 and 28). (C) 2007 Elsevier Inc. All rights reserved. C1 [Lillis, Robert J.; Mitchell, David L.; Brain, David A.; Lin, Robert P.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Bougher, Stephen W.] Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA. [Acuna, Mario H.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Lillis, RJ (reprint author), Univ Calif Berkeley, Space Sci Lab, 7 Gauss Way, Berkeley, CA 94720 USA. EM rlillis@ssl.berkeley.edu RI Bougher, Stephen/C-1913-2013; Lillis, Robert/A-3281-2008 OI Bougher, Stephen/0000-0002-4178-2729; Lillis, Robert/0000-0003-0578-517X NR 47 TC 16 Z9 16 U1 0 U2 2 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 J9 ICARUS JI Icarus PD APR PY 2008 VL 194 IS 2 BP 562 EP 574 DI 10.1016/j.icarus.2007.09.031 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 284DM UT WOS:000254685900013 ER PT J AU Lillis, RJ Frey, HV Manga, M Mitchell, DL Lin, RP Acuna, MH Bougher, SW AF Lillis, Robert J. Frey, Herbert V. Manga, Michael Mitchell, David L. Lin, Robert P. Acuna, Mario H. Bougher, Stephen W. TI An improved crustal magnetic field map of Mars from electron reflectometry: Highland volcano magmatic history and the end of the martian dynamo SO ICARUS LA English DT Article DE Mars; magnetic fields; cratering; Mars, interior; volcanism ID IMPACT EXCITATION; CASCADE RANGE; SYRTIS MAJOR; CONSTRAINTS; EVOLUTION; REGION; ARGON; RATES; ANOMALIES; CRATERS AB We apply improved kinetic modeling of electron transport in the martian thermosphere to fit pitch angle distributions measured by the Mars Global Surveyor (MGS) Magnetometer/Electron Reflectometer (MAG/ER), together with appropriate filtering, binning, averaging and error correction techniques, to create the most reliable ER global map to date of crustal magnetic field magnitude at 185 km altitude, with twice the spatial resolution and considerably higher sensitivity to crustal fields than global maps of magnetic field components produced with MAG data alone. This map compares favorably to sparsely sampled dayside MAG data taken at similar altitudes, insofar as a direct comparison is meaningful. Using this map, we present two case studies. The first compares the magnetic signatures of two highland volcanoes, concluding that the comparatively greater thermal demagnetization at Syrtis Major compared with Tyrrhena Patera is likely due to a higher ratio of intruded to extruded magmas. The second uses the map along with topographic data to compare the magnetic signatures and crater retention ages of the demagnetized Hellas impact basin and magnetized Ladon impact basin. From this comparison, we determine that the martian global dynamo magnetic field went from substantial to very weak or nonexistent in the absolute model age time interval 4.15 +/- 0.05 to 4.07 +/- 0.05 Ga ago. (C) 2007 Elsevier Inc. All rights reserved. C1 [Lillis, Robert J.; Mitchell, David L.; Lin, Robert P.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Frey, Herbert V.; Acuna, Mario H.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Manga, Michael] Univ Calif Berkeley, Dept Earth & Planetary Sci, Berkeley, CA 94720 USA. [Bougher, Stephen W.] Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA. RP Lillis, RJ (reprint author), Univ Calif Berkeley, Space Sci Lab, 7 Gauss Way, Berkeley, CA 94720 USA. EM rlillis@ssl.berkeley.edu RI Bougher, Stephen/C-1913-2013; Manga, Michael/D-3847-2013; Lillis, Robert/A-3281-2008; OI Bougher, Stephen/0000-0002-4178-2729; Lillis, Robert/0000-0003-0578-517X; Manga, Michael/0000-0003-3286-4682 NR 78 TC 66 Z9 68 U1 0 U2 3 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 J9 ICARUS JI Icarus PD APR PY 2008 VL 194 IS 2 BP 575 EP 596 DI 10.1016/j.icarus.2007.09.032 PG 22 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 284DM UT WOS:000254685900014 ER PT J AU Chambers, LS Cuzzi, JN Asphaug, E Colwell, J Sugita, S AF Chambers, Lindsey S. Cuzzi, Jeffrey N. Asphaug, Erik Colwell, Joshua Sugita, Seiji TI Hydrodynamical and radiative transfer modeling of meteoroid impacts into Saturn's rings SO ICARUS LA English DT Article DE planetary rings; Saturn; impact processes; radiative transfer ID MOVING PLASMA CLOUDS; PLANETARY RINGS; HYPERVELOCITY IMPACTS; IMAGING SCIENCE; SPOKE FORMATION; VAPOR CLOUDS; LIGHT FLASH; B-RING; BOMBARDMENT; SYSTEM AB In a small hypervelocity impact, superheated gas and particles glow brightly with thermal emission for a brief time interval at short wavelengths; this phenomenon is referred to as an impact flash. Over the past decade, impact flashes have been observed on the Moon and in the laboratory in both the IR and visible portions of the spectrum. These phenomena have been used to constrain impactor parameters, such as impact size, velocity and composition. With the arrival of the Cassini spacecraft at Saturn, we embarked on a study of impact flashes in Saturn's rings. We present results on the feasibility of observing impact flashes and therefore estimating the flux of meteoroids impacting Saturn's rings using Cassini's Ultraviolet Imaging Spectrograph (UVIS). Our modeling effort is two-fold. We start by simulating impacts using the CTH hydrodynamical code. Impacts involve an icy ring particle and a serpentine meteoroid, modeled with the ANEOS equation of state. The objects are centimeters to meters in diameter and collide at 30 to 50 km s(-1). We then use the resulting temperatures and densities of the impact plumes in a radiative transfer calculation. We calculate bound-free, free-free, electron scattering and negative ion opacities along a line-of-sight through the center of each impact plume. Our model has shown that impact flashes will not be seen with the UVIS because (1) the plumes are optically thick when their central temperatures are high, with photosphere temperatures too cool to emit observable UV flux and (2) when the plumes become optically thin, even the hottest region of the plume is too cool to observe in the UV. This corroborates the lack of UVIS impact flash detections to date. Impact flashes are not likely to be seen by other Cassini instruments because of the short lifetimes of the plumes. (C) 2007 Elsevier Inc. All rights reserved. C1 [Chambers, Lindsey S.; Asphaug, Erik] Univ Calif Santa Cruz, Dept Earth & Planetary Sci, Santa Cruz, CA 95064 USA. [Cuzzi, Jeffrey N.] NASA, Ames Res Ctr, Div Space Sci, Moffett Field, CA 94035 USA. [Colwell, Joshua] Univ Cent Florida, Dept Phys, Orlando, FL 32816 USA. [Sugita, Seiji] Univ Tokyo, Grad Sch Frontier Sci, Dept Complexity Sci & Engn, Chiba 2778561, Japan. RP Chambers, LS (reprint author), Univ Calif Santa Cruz, Dept Earth & Planetary Sci, 1156 High St, Santa Cruz, CA 95064 USA. EM lchambers@pmc.ucsc.edu NR 77 TC 8 Z9 8 U1 0 U2 0 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 J9 ICARUS JI Icarus PD APR PY 2008 VL 194 IS 2 BP 623 EP 635 DI 10.1016/j.icarus.2007.11.017 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 284DM UT WOS:000254685900017 ER PT J AU Alvarellos, JL Zahnle, KJ Dobrovolskis, AR Hamill, P AF Alvarellos, Jose Luis Zahnle, Kevin J. Dobrovolskis, Anthony R. Hamill, Patrick TI Transfer of mass from Io to Europa and beyond due to cometary impacts SO ICARUS LA English DT Article DE Io; Europa; cratering; impact processes ID CRATERING RATES; SATURN SYSTEM; EJECTA; SATELLITES; PLANETS; ORIGIN; BODIES AB We simulate the production and orbital evolution of escaping ejecta due to cometary impacts on Io. The model includes the-four Galilean satellites. Amalthea, Thebe, Jupiter's gravitational moments, Saturn and the Sun. Five scenarios are examined: an impact at the apex, the sub-jovian point. the anti-jovian point, the antapex, and at the south pole of Io. We estimate that on average a cometary impact injects thrice its mass (in the form of Io surface material) into jovicentric orbit. The majority of the escaping debris comes back to Io, but a sizeable fraction (between 5.0 and 8.7%) manages to reach Europa, and a smaller fraction Ganymede (between 1.5 and 4.6%). Smaller fractions reached Amalthea Thebe, Callisto, and Jupiter itself. For million year time scales, the mass transfer to Europa is estimated as 1.8-3.1 x 10(14) g/Myr. The median time for transfer of ejecta from Io to Europa is similar to 56 years. (C) 2007 Elsevier Inc. All rights reserved. C1 [Alvarellos, Jose Luis] Space Syst Loral, Palo Alto, CA 94303 USA. [Zahnle, Kevin J.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Dobrovolskis, Anthony R.] Univ Calif Santa Cruz, Univ Calif Observ, Lick Observ, Santa Cruz, CA 95064 USA. [Hamill, Patrick] San Jose State Univ, Dept Phys, San Jose, CA 95192 USA. RP Alvarellos, JL (reprint author), Space Syst Loral, 3825 Fabian Way,MS G-76, Palo Alto, CA 94303 USA. EM alvarellosjose@ssd.loral.com NR 34 TC 10 Z9 10 U1 0 U2 4 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 J9 ICARUS JI Icarus PD APR PY 2008 VL 194 IS 2 BP 636 EP 646 DI 10.1016/j.icarus.2007.09.025 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 284DM UT WOS:000254685900018 ER PT J AU Zahnle, K Alvarellos, JL Dobrovolskis, A Hamill, P AF Zahnle, Kevin Alvarellos, Jose L. Dobrovolskis, Anthony Hamill, Patrick TI Secondary and sesquinary craters on Europa SO ICARUS LA English DT Article DE impact processes; cratering; Io; Europa; Jupiter, satellites ID GALILEAN SATELLITES; EJECTA; FRAGMENTS; SURFACES; COMETS; SYSTEM; RATES AB We address impact cratering on Io and Europa, with the emphasis on the origin of small craters on Europa as secondary to the primary impacts of comets on In, Europa, and Ganymede. In passing we also address the origin of secondary craters generated by Zunil, a well-studied impact crater on Mars that is a plausible analog to impact craters on Io. At nominal impact rates, and taking volcanic resurfacing into account, we find that there should be 1.3 impact craters on Io, equally likely to be of any diameter between 100 m and 20 km. The corresponding model age of Europa's surface is between 60 and 100 Ma. This range of ages does not include a factor three uncertainty stemming from the uncertain sizes and numbers of comets. The mass of basaltic impact ejecta from Io to reach Europa is found to meet or exceed the micrometeoroid flux as a source of rock-forming elements to Europa's ice crust. To describe impact ejecta in more detail we adapt models for impact-generated spalls and Grady-Kipp fragments originally developed by Melosh. Our model successfully reproduces the observed size-number distributions of small craters on both Mars and Europa. However, the model predicts that a significant fraction of the 200-500 m, diameter craters on Europa are not traditional secondary craters but are instead sesquinary craters caused by impact ejecta from Io that had gone into orbit about Jupiter. This prediction is not supported by observation, which implies that high speed spalls usually break up into smaller fragments that make smaller sesquinary craters. logenic basalts are also interesting because they provide stratigraphic horizons on Europa that in principle could be used to track historic motions of the ice. and they provide materials suitable to radiometric dating of Europa's surface. (C) 2007 Elsevier Inc. All rights reserved. C1 [Zahnle, Kevin] NASA, Ames Res Ctr, Div Space Sci, Moffett Field, CA 94035 USA. [Alvarellos, Jose L.] Space Syst Loral, Palo Alto, CA 94303 USA. [Dobrovolskis, Anthony] Univ Calif Santa Cruz, Univ Calif Observ, Lick Observ, Santa Cruz, CA 95064 USA. [Hamill, Patrick] San Jose State Univ, Dept Phys, San Jose, CA 95192 USA. RP Zahnle, K (reprint author), NASA, Ames Res Ctr, Div Space Sci, MS 245-3, Moffett Field, CA 94035 USA. EM kevin.j.zahnle@nasa.gov NR 34 TC 30 Z9 30 U1 0 U2 8 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 J9 ICARUS JI Icarus PD APR PY 2008 VL 194 IS 2 BP 660 EP 674 DI 10.1016/j.icarus.2007.10.024 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 284DM UT WOS:000254685900020 ER PT J AU Radebaugh, J Loren, RD Lunine, JI Wall, SD Boubin, G Reffet, E Kirk, RL Lopes, RM Stofan, ER Soderblom, L Allison, M Janssen, M Paillou, P Callahan, P Spencer, C AF Radebaugh, J. Loren, R. D. Lunine, J. I. Wall, S. D. Boubin, G. Reffet, E. Kirk, R. L. Lopes, R. M. Stofan, E. R. Soderblom, L. Allison, M. Janssen, M. Paillou, P. Callahan, P. Spencer, C. CA Cassini Radar Team TI Dunes on Titan observed by Cassini Radar SO ICARUS LA English DT Article DE Titan; satellites, surfaces; Saturn, satellites ID LONGITUDINAL DUNES; SEDIMENT TRANSPORT; GENERAL-CIRCULATION; HUYGENS PROBE; SURFACE; WINDS; VENUS; PREDICTIONS; ATMOSPHERE; SIMULATION AB Thousands of longitudinal dunes have recently been discovered by the Titan Radar Mapper on the surface of Titan. These are found mainly within +/-30 degrees of the equator in optically-, near-infrared-, and radar-dark regions, indicating a strong proportion of organics, and cover well over 5% of Titan's surface. Their longitudinal duneform, interactions with topography, and correlation with other aeolian forms indicate a single, dominant wind direction aligned with the dune axis plus lesser, off-axis or seasonally alternating winds. Global compilations of dune orientations reveal the mean wind direction is dominantly eastwards, with regional and local variations where winds are diverted around topographically high features, such as mountain blocks or broad landforms. Global winds may carry sediments from high latitude regions to equatorial regions, where relatively drier conditions prevail, and the particles are reworked into dunes, perhaps on timescales of thousands to tens of thousands of years. On Titan, adequate sediment supply, sufficient wind, and the absence of sediment carriage and trapping by fluids are the dominant factors in the presence of dunes. (C) 2007 Elsevier Inc. All rights reserved. C1 [Radebaugh, J.; Spencer, C.] Brigham Young Univ, Dept Geol Sci, Provo, UT 84602 USA. [Loren, R. D.] Johns Hopkins Univ, Dept Space, Planetary Explorat Grp, Laurel, MD 20723 USA. [Lunine, J. I.; Boubin, G.] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA. [Wall, S. D.; Lopes, R. M.; Janssen, M.; Callahan, P.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Reffet, E.] Observ Paris, LESIA, F-92195 Meudon, France. [Kirk, R. L.; Soderblom, L.] Lowell Observ, Astrogeol Div, Flagstaff, AZ 86001 USA. [Stofan, E. R.] Proxemy Res, Bowie, MD 20715 USA. [Allison, M.] Goddard Inst Space Studies, New York, NY 10025 USA. [Paillou, P.] Observ Aquatain Sci Univers, UMR 5804, Floirac, France. RP Radebaugh, J (reprint author), Brigham Young Univ, Dept Geol Sci, Provo, UT 84602 USA. EM jani.radebaugh@byu.edu RI Lorenz, Ralph/B-8759-2016; Lopes, Rosaly/D-1608-2016; OI Lorenz, Ralph/0000-0001-8528-4644; Lopes, Rosaly/0000-0002-7928-3167; Spencer, Christopher/0000-0003-4264-3701 NR 62 TC 99 Z9 99 U1 1 U2 10 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 EI 1090-2643 J9 ICARUS JI Icarus PD APR PY 2008 VL 194 IS 2 BP 690 EP 703 DI 10.1016/j.icarus.2007.10.015 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 284DM UT WOS:000254685900022 ER PT J AU Zebker, HA Wye, LC Janssen, MA AF Zebker, Howard A. Wye, Lauren C. Janssen, Michael A. CA Cassini Radar Team TI Titan's surface from reconciled Cassini microwave reflectivity and emissivity observations SO ICARUS LA English DT Article DE Titan; radar observations; satellites, surfaces ID THERMAL EMISSION; RADAR; APPROXIMATION; POLARIZATION; ROUGHNESS AB The surface of Titan, Saturn's largest moon, appears to consist of solid hydrocarbons or CO2 with considerable small-scale structure, according to a new electromagnetic scattering model that uses both Cassini radar reflectivity and emissivity measurements. Our model resolves a well-known ambiguity in active and passive observations of surfaces, namely that the dielectric constant retrieved from radiometric data is usually less than that obtained from radar backscatter analysis. We present here parameters of Titan derived from radar and radiometric responses using a single set of surface physical descriptors. The observed dielectric constant ranges from 1.75-2.5, consistent with the solids above, but also with unconsolidated water or water/ammonia ice. Inferred rms slopes of the surface range from 10 degrees-16 degrees at Cassini's 2.2 cm-lambda, with radar albedos of about 30%. Emissivities of the surface are quite high, on the order of 90%. We find that the majority of the backscattered radar energy results from volume, rather than surface, scattering processes. Thus large-scale variations in radar brightness are mainly diagnostic of composition and structure within Titan's near subsurface. The high level of volume scatter (about 15% of incident energy) and consequent high radar albedo suggest significant wavelength-scale structure and multiple scatter within the medium. This is most consistent with a surface composed either of ubiquitous mm-size bubbles within the "ice," analogous to a vesicular cryolava, or structures similar to ice pipes and lenses found in terrestrial ice sheets. The cryovolcanic hypothesis suggests planet-wide resurfacing by active volcanism to explain the large-scale uniformity of observed backscatter. If the lens/pipe mechanism pertains, it can imply percolation of precipitating liquid or surface melt through the Titan "firn." (C) 2007 Elsevier Inc. All rights reserved. C1 [Zebker, Howard A.; Wye, Lauren C.] Stanford Univ, Dept Geophys, Stanford, CA 94305 USA. [Zebker, Howard A.; Wye, Lauren C.] Stanford Univ, Dept Elect Engn, Stanford, CA 94305 USA. [Janssen, Michael A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Cassini Radar Team] CALTECH, Jet Prop Lab, Cassini Project, Pasadena, CA 91109 USA. RP Zebker, HA (reprint author), Stanford Univ, Dept Geophys, Stanford, CA 94305 USA. EM zebker@stanford.edu NR 26 TC 17 Z9 17 U1 0 U2 4 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 J9 ICARUS JI Icarus PD APR PY 2008 VL 194 IS 2 BP 704 EP 710 DI 10.1016/j.icarus.2007.10.019 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 284DM UT WOS:000254685900023 ER PT J AU Rappaport, NJ Iess, L Wahr, J Lunine, JI Armstrong, JW Asmar, SW Tortora, P Di Benedetto, M Racioppa, P AF Rappaport, Nicole J. Iess, Luciano Wahr, John Lunine, Jonathan I. Armstrong, J. W. Asmar, Sami W. Tortora, Paolo Di Benedetto, Mauro Racioppa, Paolo TI Can Cassini detect a subsurface ocean in Titan from gravity measurements? SO ICARUS LA English DT Article DE Titan; interiors ID INTERNAL STRUCTURE; TIDAL RESPONSE; HIGH-PRESSURE; SURFACE; DYNAMICS; ROTATION; ORIGIN; METHANE; EUROPA; EARTH AB Recent models of Titan's interior predict that the satellite contains an ocean of water and ammonia under an icy layer. Direct evidence for the presence of an ocean can be provided on the Cassini mission only by radio science determination of Titan Love number k(2). Simulations that use the five flybys T11, T22 T33, T45, and T68 (the latter two belonging to the extended mission) lead to the result that in the elastic case, where the Love number is real, k(2) will be determined with a one-sigma accuracy of 0.1. In the viscoelastic case, where k(2) is complex, the real and imaginary parts of k(2) will be determined with one sigma accuracies of 0.138 and 0.115, respectively. Ocean and oceanless models that include a viscoelastic theology are built. In the viscoelastic case, there is a 93% probability to correctly predict the presence or absence of an ocean; this probability improves to 97% in the elastic case. (C) 2007 Elsevier Inc. All rights reserved. C1 [Rappaport, Nicole J.; Armstrong, J. W.; Asmar, Sami W.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Iess, Luciano; Di Benedetto, Mauro; Racioppa, Paolo] Univ Roma La Sapienza, Dipartimento Ingn Aerospaziale Astronaut, I-00184 Rome, Italy. [Wahr, John] Univ Colorado, Dept Phys, Boulder, CO 80309 USA. [Lunine, Jonathan I.] INAF IFSI, I-00133 Rome, Italy. [Lunine, Jonathan I.] Lunar & Planetary Lab, Tucson, AZ 85721 USA. [Tortora, Paolo] Univ Bologna, DIEM, Fac Engn 2, I-47100 Forli, Italy. RP Rappaport, NJ (reprint author), CALTECH, Jet Prop Lab, MS 301-150,4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM nicole.j.rappaport@jpl.nasa.gov RI IESS, Luciano/F-4902-2011; Tortora, Paolo/J-6191-2012 OI IESS, Luciano/0000-0002-6230-5825; Tortora, Paolo/0000-0001-9259-7673 NR 30 TC 21 Z9 21 U1 0 U2 2 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 J9 ICARUS JI Icarus PD APR PY 2008 VL 194 IS 2 BP 711 EP 720 DI 10.1016/j.icarus.2007.11.024 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 284DM UT WOS:000254685900024 ER PT J AU Anderson, CM Young, EF Chanover, NJ Mckay, CP AF Anderson, C. M. Young, E. F. Chanover, N. J. McKay, C. P. TI HST spectral imaging of Titan's haze and methane profile between 0.6 and 1 mu m during the 2000 opposition SO ICARUS LA English DT Article DE Titan; atmospheres, structure; radiative transfer ID NORTH POLAR STRATOSPHERE; TROPOSPHERIC CLOUDS; LOWER ATMOSPHERE; SURFACE; AEROSOLS; MODEL; ALBEDO; REANALYSIS; ABUNDANCES; WINDS AB We report on the analysis of high spatial resolution visible to near-infrared spectral images of Titan at L-s = 240 degrees in November 2000, obtained with the Space Telescope Imaging Spectrograph instrument on board the Hubble Space Telescope as pan of program GO-8580. We employ a radiative transfer fractal particle aerosol model with a Bayesian parameter estimation routine that computes Titan's absolute reflectivity per pixel for 122 wavelengths by modeling the vertical distribution of the lower atmosphere haze and tropospheric methane. Analysis of these data suggests that Titan's haze concentration in the lower atmosphere varies in strength with latitude. We find Titan's tropospheric methane profile to be fairly consistent with latitude and longitude, and we find evidence for local areas of a CH4-N-2 binary saturation in Titan's troposphere. Our results suggest that a methane and haze profile at one location on Titan would not be representative of global conditions. (C) 2007 Elsevier Inc. All rights reserved. C1 [Anderson, C. M.] NASA, Goddard Space Flight Ctr, Solar Syst Explorat Div, Greenbelt, MD 20771 USA. [Anderson, C. M.] New Mexico State Univ, Dept Astron, Las Cruces, NM 88003 USA. [Young, E. F.] SW Res Inst, Dept Space Sci, Boulder, CO 80302 USA. NASA, Ames Res Ctr, Div Space Sci, Moffett Field, CA 94035 USA. RP Anderson, CM (reprint author), NASA, Goddard Space Flight Ctr, Solar Syst Explorat Div, Code 661, Greenbelt, MD 20771 USA. EM carrie.anderson@gsfc.nasa.gov RI Anderson, Carrie/C-8097-2012 NR 54 TC 8 Z9 8 U1 0 U2 5 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 J9 ICARUS JI Icarus PD APR PY 2008 VL 194 IS 2 BP 721 EP 745 DI 10.1016/j.icarus.2007.11.008 PG 25 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 284DM UT WOS:000254685900025 ER PT J AU Ipatov, SI Kutyrev, AS Madsen, GJ Mather, JC Moseley, SH Reynolds, RJ AF Ipatov, Sergei I. Kutyrev, Alexander S. Madsen, Greg J. Mather, John C. Moseley, S. Harvey Reynolds, Ronald J. TI Dynamical zodiacal cloud models constrained by high resolution spectroscopy of the zodiacal light SO ICARUS LA English DT Article DE asteroids; comets, dust; trans-neptunian objects; spectroscopy; zodiacal light ID INTERPLANETARY DUST PARTICLES; FRAUNHOFER LINE-PROFILES; KUIPER-BELT DUST; RADIAL-VELOCITY MEASUREMENTS; TRANS-NEPTUNIAN OBJECTS; SOLAR-SYSTEM DUST; NEAR-EARTH SPACE; TERRESTRIAL PLANETS; ORBITAL EVOLUTION; COSMIC DUST AB The simulated Doppler shifts of the solar Mg I Fraunhofer line produced by scattering on the solar light by asteroidal, cometary, and trans-neptunian dust particles are compared with the shifts obtained by Wisconsin H-Alpha Mapper (WHAM) spectrometer. The simulated spectra are based on the results of integrations of the orbital evolution of particles under the gravitational influence of planets, the Poynting-Robertson drag, radiation pressure, and solar wind drag. Our results demonstrate that the differences in the line centroid position in the solar elongation and in the line width averaged over the elongations for different sizes of particles are usually less than those for different sources of dust. The deviation of the derived spectral parameters for various sources of dust used in the model reached maximum at the elongation (measured eastward from the Sun) between 90 degrees and 120 degrees. For the future zodiacal light Doppler shifts measurements, it is important to pay a particular attention to observing at this elongation range. At the elongations of the fields observed by WHAM, the model-predicted Doppler shifts were close to each other for several scattering functions considered. Therefore the main conclusions of our paper do not depend on a scattering function and mass distribution of particles if they are reasonable. A comparison of the dependencies of the Doppler shifts on solar elongation and the mean width of the Mg I line modeled for different sources of dust with those obtained from the WHAM observations shows that the fraction of cometary particles in zodiacal dust is significant and can be dominant. Cometary particles originating inside Jupiter's orbit and particles originating beyond Jupiter's orbit (including trans-neptunian dust particles) can contribute to zodiacal dust about 1/3 each, with a possible deviation from 1/3 up to 0.1-0.2. The fraction of asteroidal dust is estimated to be similar to 0.3-0.5. The mean eccentricities of zodiacal particles located at 1-2 AU from the Sun that better fit the WHAM observations are between 0.2 and 0.5, with a more probable value of about 0.3. (C) 2007 Elsevier Inc. All rights reserved. C1 [Ipatov, Sergei I.] Carnegie Inst Washington, Dept Terr Magnetism, Washington, DC 20015 USA. [Ipatov, Sergei I.] Moscow Space Res Inst, Moscow 117997, Russia. [Kutyrev, Alexander S.; Mather, John C.; Moseley, S. Harvey] NASA, GSFC, Greenbelt, MD 20771 USA. [Madsen, Greg J.] Anglo Australian Observ, Epping, NSW 1710, Australia. [Reynolds, Ronald J.] Univ Wisconsin, Dept Astron, Madison, WI 53706 USA. RP Ipatov, SI (reprint author), Carnegie Inst Washington, Dept Terr Magnetism, 5241 Broad Branch Rd, Washington, DC 20015 USA. EM siipatov@hotmail.com RI Ipatov, Sergei/O-2302-2014 OI Ipatov, Sergei/0000-0002-1413-9180 NR 77 TC 11 Z9 11 U1 0 U2 2 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 J9 ICARUS JI Icarus PD APR PY 2008 VL 194 IS 2 BP 763 EP 782 DI 10.1016/j.icarus.2007.11.009 PG 20 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 284DM UT WOS:000254685900028 ER PT J AU Nna-Mvondo, D Khare, B Ishihara, T McKay, CP AF Nna-Mvondo, Delphine Khare, Bishun Ishihara, Tomoko McKay, Christopher P. TI Experimental impact shock chemistry on planetary icy satellites SO ICARUS LA English DT Review DE ices; impact processes; prebiotic chemistry ID PROTON IRRADIATED H2O+CO2; HUBBLE-SPACE-TELESCOPE; WATER-ICE; HYPERVELOCITY IMPACT; ORGANIC-MOLECULES; HYDROGEN-PEROXIDE; GALILEAN SATELLITES; COMETARY DELIVERY; AMINO-ACIDS; ULTRAVIOLET PHOTOLYSIS AB We present new experimental results on impact shock chemistry into icy satellites of the outer planets. Icy mixtures of pure water ice with CO(2), Na(2)CO(3), CH(3)OH, and CH(3)OH/(NH(4))(2)SO(4) at 77 K were ablated with a powerful pulsed laser-a new technique used to simulate shock processes which can occur during impacts. New products were identified by GC-MS and FTIR analyses after laser ablation. Our results show that hydrogen peroxide is formed in irradiated H(2)O/CO(2) ices with a final concentration of 0.23%. CO and CH(3)OH were also detected as main products. The laser ablation of frozen H(2)O/Na(2)CO(3) generates only CO and CO(2) as destruction products from the salt. Pulsed irradiation of water ice containing methanol leads also to the formation of CO and CO(2), generates methane and more complex molecules containing carbonyl groups like acetaldehyde, acetone, methyl formate, and a diether, dimethyl formal. The last three compounds are also produced when adding ammonium sulfate to H(2)O/CH(3)OH ice, but acetone is more abundant. The formation of two hydrocarbons, CH(4) and C(2)H(6) is observed as well as the production of three nitrogen compounds, nitrous oxide, hydrogen cyanide, and acetonitrile. (C) 2007 Elsevier Inc. All fights reserved. C1 [Nna-Mvondo, Delphine; Khare, Bishun; Ishihara, Tomoko; McKay, Christopher P.] NASA, Ames Res Ctr, Div Space Sci, Moffett Field, CA 94035 USA. [Khare, Bishun; Ishihara, Tomoko] NASA, Ames Res Ctr, SETI Inst, Moffett Field, CA 94035 USA. RP Nna-Mvondo, D (reprint author), Inst Nacl Tecn Aeroespacial, Ctr Astrobiol, CSIC INTA, Planetary Geol Lab, Carretera Ajalvir,Km 4, Madrid 28850, Spain. EM nnamvondod@inta.es NR 113 TC 15 Z9 15 U1 1 U2 13 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 J9 ICARUS JI Icarus PD APR PY 2008 VL 194 IS 2 BP 816 EP 829 DI 10.1016/j.icarus.2007.11.001 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 284DM UT WOS:000254685900032 ER PT J AU Hodyss, R Johnson, PV Orzechowska, GE Goguen, JD Kanik, I AF Hodyss, Robert Johnson, Paul V. Orzechowska, Grazyna E. Goguen, Jay D. Kanik, Isik TI Carbon dioxide segregation in 1 : 4 and 1 : 9 CO2 : H2O ices SO ICARUS LA English DT Article DE ices; ices, IR spectroscopy; satellites, surfaces; photochemistry ID SOLAR-SYSTEM BODIES; WATER-ICE; ASTROPHYSICAL IMPLICATIONS; INFRARED SPECTRUM; BAND STRENGTHS; CO2; SPECTROMETER; SPECTROSCOPY; MIXTURES; SURFACE AB The mid-infrared spectra of mixed vapor deposited ices of CO2 and H2O were studied as a function of both deposition temperature and warming from 15 to 100 K. The spectra of ices deposited at 15 K show marked changes on warming beginning at 60 K. These changes are consistent with CO2 segregating within the ice matrix into pure CO2 domains. Ices deposited at 60 and 70 K show a greater degree of segregation, as high as 90% for 1:4 CO2:H2O ice mixtures deposited at 70 K. As the ice is warmed above 80 K, preferential sublimation of the segregated CO2 is observed. The kinetics of the segregation process is also examined. The segregation of the CO2 as the ice is warmed corresponds to temperatures at which the structure of the water ice matrix changes from the high density amorphous phase to the low density amorphous phase. We show how these microstructural changes in the ice have a profound effect on the photochemistry induced by ultraviolet irradiation. These experimental results provide a framework in which observations of CO2 on the icy bodies of the outer Solar System can be considered. (C) 2007 Elsevier Inc. All rights reserved. C1 [Hodyss, Robert; Johnson, Paul V.; Orzechowska, Grazyna E.; Goguen, Jay D.; Kanik, Isik] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Hodyss, R (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM robert.p.hodyss@jpl.nasa.gov RI Johnson, Paul/D-4001-2009 OI Johnson, Paul/0000-0002-0186-8456 NR 39 TC 10 Z9 10 U1 1 U2 11 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 J9 ICARUS JI Icarus PD APR PY 2008 VL 194 IS 2 BP 830 EP 836 DI 10.1016/j.icarus.2007.10.005 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 284DM UT WOS:000254685900033 ER PT J AU Noor, AK Venneri, SL AF Noor, Ahmed K. Venneri, Samuel L. TI ISE: Intelligent Synthesis Environment for future aerospace systems SO IEEE AEROSPACE AND ELECTRONIC SYSTEMS MAGAZINE LA English DT Article AB The Intelligent Synthesis Environment (ISE) being developed by NASA, UVA, and JPL for significantly enhancing the rapid creation of innovative affordable products and missions is described. ISE uses a synergistic combination of leading-edge technologies, including high-performance computing, high-capacity communications and networking, virtual product development, knowledge-based engineering, computational intelligence, human-computer interaction, and product information management. The environment will link scientists, design teams, manufacturers, suppliers, and consultants who participate in the mission synthesis, as well as in the creation and operation of the aerospace system. It will radically advance the process by which complex science missions are synthesized, and high-tech engineering systems are designed, manufactured, and operated. The evolution of engineering design is described along with the shortcomings of current product development techniques. The need for ISE to create high-science payoff missions and aerospace systems at affordable costs is discussed. The five major components critical to ISE and some of their sub-elements are described: namely, human-ISE interaction; infrastructure for distributed collaboration; rapid synthesis and simulation tools; intelligent life-cycle system integration; and cultural change in the creative process. Related government and industry programs are outlined and future impact of ISE on complex missions and aerospace systems is discussed. C1 [Noor, Ahmed K.] Univ Virginia, Ctr Adv Computat Technol, Langley Res Ctr, NASA, Hampton, VA 23681 USA. [Venneri, Samuel L.] NASA Headquarters, Washington, DC 20546 USA. RP Noor, AK (reprint author), Univ Virginia, Ctr Adv Computat Technol, Langley Res Ctr, NASA, Hampton, VA 23681 USA. NR 10 TC 1 Z9 1 U1 0 U2 2 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855 USA SN 0885-8985 J9 IEEE AERO EL SYS MAG JI IEEE Aerosp. Electron. Syst. Mag. PD APR PY 2008 VL 23 IS 4 BP 31 EP 44 DI 10.1109/MAES.2008.4493440 PG 14 WC Engineering, Aerospace; Engineering, Electrical & Electronic SC Engineering GA 332HX UT WOS:000258075200006 ER PT J AU Gitelson, AA Vina, A Masek, JG Verma, SB Suyker, AE AF Gitelson, Anatoly A. Vina, Andres Masek, Jeffrey G. Verma, Shashi B. Suyker, Andrew E. TI Synoptic monitoring of gross primary productivity of maize using Landsat data SO IEEE GEOSCIENCE AND REMOTE SENSING LETTERS LA English DT Article DE optical imaging; remote sensing; vegetation mapping ID NET PRIMARY PRODUCTION; LIGHT-USE EFFICIENCY; TERRESTRIAL GROSS; VEGETATION INDEX; CO2 EXCHANGE; EOS-MODIS; REFLECTANCE; ECOSYSTEM; CHLOROPHYLL; MODEL AB There is a growing interest in monitoring the gross primary productivity (GPP) of crops due mostly to their carbon sequestration potential. Both within- and between-field variability are important components of crop GPP monitoring, particularly for the estimation of carbon budgets. In this letter, we present a new technique for daytime GPP estimation in maize based,on the close and consistent relationship between GPP and crop chlorophyll content, and entirely on remotely sensed data. A recently proposed chlorophyll index (CI), which involves green and near-infrared spectral bands, was used to retrieve daytime GPP from Landsat Enhanced Thematic Mapper Plus (ETM+) data. Because of its high spatial resolution (i.e., 30 x 30 m/pixel), this satellite system is particularly appropriate for detecting not only between- but also within-field GPP variability during the growing season. The CI obtained using atmospherically corrected Landsat ETM+ data was found to be linearly related with daytime maize GPP: root mean squared error of less than 1.58 gC.m(-2).d(-1) in a GPP range of 1.88 to 23.1 gC.m(-2).d(-1); therefore, it constitutes an accurate surrogate measure for GPP estimation. For comparison purposes, other vegetation indices were also tested. These results open new possibilities for analyzing the spatiotemporal variation of the GPP of crops using the extensive archive of Landsat imagery acquired since the early 1980s. C1 [Gitelson, Anatoly A.; Verma, Shashi B.; Suyker, Andrew E.] Univ Nebraska, Sch Nat Resources, Lincoln, NE 68588 USA. [Vina, Andres] Michigan State Univ, Dept Fisheries & Wildlife, Ctr Syst Integrat & Sustainabil, E Lansing, MI 48824 USA. [Masek, Jeffrey G.] NASA, Goddard Space Flight Ctr, Biospher Sci Branch, Greenbelt, MD 20771 USA. RP Gitelson, AA (reprint author), Univ Nebraska, Sch Nat Resources, Lincoln, NE 68588 USA. RI Masek, Jeffrey/D-7673-2012; Gitelson, Anatoly/G-3452-2012 FU NASA Land Cover and Land Use Change Program [NNG06GG17G]; U.S. Department of Energy (DoE) EPSCoR [DE-FG-02-00ER45827]; DoE Office of Science (BER) [DE-FG02-03ER63639] FX This work was supported by in part by the NASA Land Cover and Land Use Change Program under Grant NNG06GG17G, in part by the U.S. Department of Energy (DoE) EPSCoR program under Grant DE-FG-02-00ER45827 and the DoE Office of Science (BER) under Grant DE-FG02-03ER63639, and in part by the Hatch Act. NR 35 TC 49 Z9 50 U1 1 U2 23 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 1545-598X J9 IEEE GEOSCI REMOTE S JI IEEE Geosci. Remote Sens. Lett. PD APR PY 2008 VL 5 IS 2 BP 133 EP 137 DI 10.1109/LGRS.2008.915598 PG 5 WC Geochemistry & Geophysics; Engineering, Electrical & Electronic; Remote Sensing; Imaging Science & Photographic Technology SC Geochemistry & Geophysics; Engineering; Remote Sensing; Imaging Science & Photographic Technology GA 342EH UT WOS:000258766900003 ER PT J AU Halthore, RN Shettle, EP Markham, BL Mango, SA AF Halthore, Rangasayi N. Shettle, Eric P. Markham, Brian L. Mango, Stephen A. TI Role of aerosol absorption in satellite sensor calibration SO IEEE GEOSCIENCE AND REMOTE SENSING LETTERS LA English DT Article DE aerosol absorption; vicarious calibration; Visible/Infrared Imager/Radiometer Suite (VIIRS) ID PERFORMANCE AB The importance of aerosol absorption in satellite sensor vicarious calibration and/or satellite measurement of physical parameters is reiterated in a sensitivity study performed using a radiative transfer model, with field-measured data as input. Broadband shortwave surface fluxes need to be measured according to new protocols, described herein, to infer atmospheric absorption to improve calibration accuracy to within the +/- 2% stated goal of next-generation sensors such as Visible/Infrared Imager/Radiometer Suite. C1 [Halthore, Rangasayi N.; Shettle, Eric P.] USN, Res Lab, Remote Sensing Div, Washington, DC 20375 USA. [Halthore, Rangasayi N.] NASA Headquarters, Washington, DC 20546 USA. [Markham, Brian L.] NASA, Goddard Space Flight Ctr, Hydrospher & Biospher Sci Lab, Greenbelt, MD 20771 USA. [Mango, Stephen A.] Natl Polar Orbiting Operat Environm Satellite Sys, Integrated Program Off, Silver Spring, MD 20910 USA. RP Halthore, RN (reprint author), USN, Res Lab, Remote Sensing Div, Washington, DC 20375 USA. RI Markham, Brian/M-4842-2013 OI Markham, Brian/0000-0002-9612-8169 FU Integrated Program Office, National Polar-orbiting Operational Environmental Satellite System; NRL FX This work was supported in part by the Integrated Program Office, National Polar-orbiting Operational Environmental Satellite System and in part by the NRL 6.1 under the in-house funding for aerosol research. NR 16 TC 0 Z9 0 U1 1 U2 3 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855 USA SN 1545-598X J9 IEEE GEOSCI REMOTE S JI IEEE Geosci. Remote Sens. Lett. PD APR PY 2008 VL 5 IS 2 BP 157 EP 161 DI 10.1109/LGRS.2008.915735 PG 5 WC Geochemistry & Geophysics; Engineering, Electrical & Electronic; Remote Sensing; Imaging Science & Photographic Technology SC Geochemistry & Geophysics; Engineering; Remote Sensing; Imaging Science & Photographic Technology GA 342EH UT WOS:000258766900008 ER PT J AU Wenny, BN Xiong, X AF Wenny, Brian N. Xiong, Xiaoxiong TI Using a cold earth surface target to characterize long-term stability of the MODIS thermal emissive bands SO IEEE GEOSCIENCE AND REMOTE SENSING LETTERS LA English DT Article DE calibration stability; Moderate Resolution Imaging Spectroradiometer (MODIS); remote sensing; thermal emissive bands (TEB) ID DOME-C; ANTARCTICA AB The Moderate Resolution Imaging Spectroradiometer (MODIS) has successfully provided Earth image products for instruments on the Terra and Aqua satellites since 2000 and 2002, respectively. Maintaining accurate radiometric calibration and calibration consistency between two sensors is an important issue for continued quality of long-term data records, especially as the instruments operate beyond their original projected mission lifetime. A strategy to use frequent MODIS measurements of the brightness temperature of the land surface in the area surrounding Dome Concordia, Antarctica (75.1 degrees S, 123.4 degrees E) to track the long-term stability of MODIS Band 31 is presented. Dome Concordia, located on the Antarctic plateau, is one of the most homogeneous land surfaces on Earth in terms of surface temperature and emissivity, with a seasonal temperature range of 190-250 K. The extremely dry, cold, and rarefied atmosphere of the site makes it ideal to track and detect any long-term changes in the MODIS thermal band response through trend analyses of near-nadir MODIS overpass data in conjunction with surface temperature measurements. Application of this approach shows an average relative bias between Terra and Aqua MODIS Band 31 (11 mu m) measurements of -0.08 K, which is well within the calibration uncertainty. C1 [Wenny, Brian N.] Sci Syst & Applicat Inc, Lanham, MD 20706 USA. [Xiong, Xiaoxiong] NASA, Goddard Space Flight Ctr, Sci & Explorat Directorate, Greenbelt, MD 20771 USA. RP Wenny, BN (reprint author), Sci Syst & Applicat Inc, Lanham, MD 20706 USA. NR 18 TC 25 Z9 25 U1 0 U2 2 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855 USA SN 1545-598X J9 IEEE GEOSCI REMOTE S JI IEEE Geosci. Remote Sens. Lett. PD APR PY 2008 VL 5 IS 2 BP 162 EP 165 DI 10.1109/LGRS.2008.915603 PG 4 WC Geochemistry & Geophysics; Engineering, Electrical & Electronic; Remote Sensing; Imaging Science & Photographic Technology SC Geochemistry & Geophysics; Engineering; Remote Sensing; Imaging Science & Photographic Technology GA 342EH UT WOS:000258766900009 ER PT J AU Zhan, XW Crow, WT Jackson, TJ O'Neill, PE AF Zhan, Xiwu Crow, Wade T. Jackson, Thomas J. O'Neill, Peggy E. TI Improving spaceborne radiometer soil moisture retrievals with alternative aggregation rules for ancillary parameters in highly heterogeneous vegetated areas SO IEEE GEOSCIENCE AND REMOTE SENSING LETTERS LA English DT Article DE microwave; remote sensing; soil moisture ID MICROWAVE; BAND AB Retrieving soil moisture from spaceborne microwave radiometer observations often requires ancillary parameters such as surface vegetation opacity or vegetation water content (VWC). The conventional approach for deriving representative footprint-scale values of these parameters is to simply average the corresponding parameters of high-resolution pixels over the entire radiometer footprint. However, previous work has shown that simple averaging of ancillary parameter values may result in biased soil moisture retrievals from spaceborne radiometers. This letter uses a synthetic observing-system simulation experiment framework to theoretically demonstrate that ancillary VWC or canopy-opacity parameter values obtained with an alternative aggregation rule may significantly reduce the magnitude of soil moisture retrieval errors for highly heterogeneous vegetated areas. C1 [Zhan, Xiwu] NOAA, Natl Environm Satellite Data & Informat Serv, Camp Springs, MD 20746 USA. [Crow, Wade T.; Jackson, Thomas J.] USDA ARS, Hydrol & Remote Sensing Lab, Beltsville, MD 20705 USA. [O'Neill, Peggy E.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Zhan, XW (reprint author), NOAA, Natl Environm Satellite Data & Informat Serv, Camp Springs, MD 20746 USA. EM xiwu.zhan@noaa.gov RI Zhan, Xiwu/F-5487-2010; O'Neill, Peggy/D-2904-2013 FU National Aeronautics and Space Administration [NAG8-1517, NAG5-6494]; National Oceanic and Atmospheric Administration [NA96GP0413] FX This work was supported in part by the National Aeronautics and Space Administration under Grants NAG8-1517 and NAG5-6494 and in part by the National Oceanic and Atmospheric Administration under Grant NA96GP0413. The views, opinions, and findings contained in this paper are those of the authors and should not be construed as an official National Oceanic and Atmospheric Administration or U.S. Government position, policy, or decision. NR 13 TC 9 Z9 9 U1 0 U2 5 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855 USA SN 1545-598X J9 IEEE GEOSCI REMOTE S JI IEEE Geosci. Remote Sens. Lett. PD APR PY 2008 VL 5 IS 2 BP 261 EP 265 DI 10.1109/LGRS.2008.915931 PG 5 WC Geochemistry & Geophysics; Engineering, Electrical & Electronic; Remote Sensing; Imaging Science & Photographic Technology SC Geochemistry & Geophysics; Engineering; Remote Sensing; Imaging Science & Photographic Technology GA 342EH UT WOS:000258766900030 ER PT J AU Durden, SL Tanelli, S AF Durden, S. L. Tanelli, S. TI Predicted effects of nonuniform beam filling on GPM radar data SO IEEE GEOSCIENCE AND REMOTE SENSING LETTERS LA English DT Article DE attenuation; meteorological radar; rain ID TRMM PRECIPITATION RADAR; RETRIEVAL; RAIN AB The Global Precipitation Measurement mission (GPM) will carry the first dual-frequency spaceborne radar (DPR) for rainfall observation. We use dual-frequency airborne radar data to simulate observations at GPM DPR resolution and frequencies and to investigate errors due to nonuniform beam filling effects. Errors at Ku-band are similar to those found in previous studies. Errors in the Ka-band path-integrated attenuation and near-surface reflectivity are larger than at Ku-band. Errors in rain-top reflectivity, where attenuation is neglected, are smaller at Ka-band than at Ku-band because the Ka-band Z-R relation is closer to being linear. C1 [Durden, S. L.; Tanelli, S.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Durden, SL (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM sdurden@jpl.nasa.gov FU NASA FX The research described here was performed at the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. Support from the NASA Precipitation Measurement Missions program is gratefully acknowledged. NR 9 TC 6 Z9 7 U1 0 U2 1 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855 USA SN 1545-598X J9 IEEE GEOSCI REMOTE S JI IEEE Geosci. Remote Sens. Lett. PD APR PY 2008 VL 5 IS 2 BP 308 EP 310 DI 10.1109/LGRS.2008.916068 PG 3 WC Geochemistry & Geophysics; Engineering, Electrical & Electronic; Remote Sensing; Imaging Science & Photographic Technology SC Geochemistry & Geophysics; Engineering; Remote Sensing; Imaging Science & Photographic Technology GA 342EH UT WOS:000258766900040 ER PT J AU Shen, SH Leptoukh, GG Acker, JG Yu, ZJ Kempler, SJ AF Shen, Suhung Leptoukh, Gregory G. Acker, James G. Yu, Zuojun Kempler, Steven J. TI Seasonal variations of chlorophyll a concentration in the northern South China Sea SO IEEE GEOSCIENCE AND REMOTE SENSING LETTERS LA English DT Article DE data management; ocean color; remote sensing ID LUZON AB Monthly climatology of chlorophyll a concentration (chl a) based on nine years of SeaWiFS data is used to illustrate seasonal variations and spatial structures in the northern South China Sea (SCS). Chl a starts to increase in September at the northern coast of Luzon Island, continues to increase in the autumn, and reaches its maximum in December or January. Maximum chl a is centered in the northern SCS off the northwestern coast of Luzon Island. Chl a starts to decrease gradually in February, and its values become very low from June to August. The region of elevated chl a during the winter bloom season is funnel shaped, with the narrow end at the northern coast of Luzon Island, where the chl a value is highest and opening toward the northwest. The sea surface temperature (SST) in this funnel-shaped region is significantly colder than SST in surrounding regions of the same latitude. The present study indicates that the winter blooms indicated by higher chl a and colder SST in the northern SCS are linked strongly to the local winter monsoon. The initial data exploration and analysis presented in this study was carried out using Giovanni, a state-of-the-art Web-based data analysis and visualization tool. C1 [Shen, Suhung] George Mason Univ, Fairfax, VA 22030 USA. [Shen, Suhung; Leptoukh, Gregory G.; Acker, James G.; Kempler, Steven J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Acker, James G.] RS Informat Syst Inc, Greenbelt, MD 20771 USA. [Yu, Zuojun] Univ Hawaii, Int Pacific Res Ctr, Honolulu, HI 96822 USA. RP Shen, SH (reprint author), George Mason Univ, Fairfax, VA 22030 USA. EM Suhung.Shen@gsfc.nasa.gov FU Goddard Earth Sciences Data and Information Services Center; National Aeronautics and Space Administration [CAN 02-OES-01]; Ocean Color Time-Series Project (PI, Watson Gregg) FX The authors gratefully acknowledge the high-quality technical support from the Giovanni team at the Goddard Earth Sciences Data and Information Services Center. This work was supported partly by the National Aeronautics and Space Administration CAN 02-OES-01, Ocean Color Time-Series Project (PI, Watson Gregg). NR 16 TC 17 Z9 19 U1 0 U2 9 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855 USA SN 1545-598X J9 IEEE GEOSCI REMOTE S JI IEEE Geosci. Remote Sens. Lett. PD APR PY 2008 VL 5 IS 2 BP 315 EP 319 DI 10.1109/LGRS.2008.915932 PG 5 WC Geochemistry & Geophysics; Engineering, Electrical & Electronic; Remote Sensing; Imaging Science & Photographic Technology SC Geochemistry & Geophysics; Engineering; Remote Sensing; Imaging Science & Photographic Technology GA 342EH UT WOS:000258766900042 ER PT J AU Radisic, V Sawdai, D Scott, D Deal, WR Dang, L Li, D Cavus, A Fung, A Samoska, L To, R Gaier, T Lai, R AF Radisic, Vesna Sawdai, Donald Scott, Dennis Deal, William R. Dang, Linh Li, Danny Cavus, Abdullah Fung, Andy Samoska, Lorene To, Richard Gaier, Todd Lai, Richard TI Demonstration of 184 and 255-GHz amplifiers using InPHBT technology SO IEEE MICROWAVE AND WIRELESS COMPONENTS LETTERS LA English DT Article DE amplifier; heterojunction bipolar transistor (HBT); MM-wave; monolithic microwave integrated circuit (MMIC); sub-millimeter wave ID G-BAND; MMIC AMPLIFIER; GHZ; 35-NM AB In this letter, 184 and 255 GHz single-stage heterojunction bipolar transistor (HBT) amplifiers are reported. Each amplifier uses a single-emitter 0.4 mu m x 15 mu m InP HBT device with maximum frequency of oscillation (f(max)) greater than 500 GHz and f(T) of similar to 200 GHz. The 183 GHz single-stage amplifier has demonstrated gain of 4.3 +/- 0.4 dB for all sites on the wafer. The 255 GHz amplifier has measured gain of 3.5 dB and demonstrates the highest frequency measured HBT amplifier gain reported to date. Both amplifiers show excellent agreement with original simulation. C1 [Radisic, Vesna; Sawdai, Donald; Scott, Dennis; Deal, William R.; Dang, Linh; Li, Danny; Cavus, Abdullah; To, Richard; Lai, Richard] Northrop Grumman Corp, Redondo Beach, CA USA. [Fung, Andy; Samoska, Lorene; Gaier, Todd] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Radisic, V (reprint author), Northrop Grumman Corp, Redondo Beach, CA USA. EM vesna@ieee.org NR 10 TC 16 Z9 16 U1 0 U2 2 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855 USA SN 1531-1309 J9 IEEE MICROW WIREL CO JI IEEE Microw. Wirel. Compon. Lett. PD APR PY 2008 VL 18 IS 4 BP 281 EP 283 DI 10.1109/LMWC.2008.918952 PG 3 WC Engineering, Electrical & Electronic SC Engineering GA 288JC UT WOS:000254981500021 ER PT J AU Wang, JR Racette, PE Pieprneier, JR AF Wang, James R. Racette, Paul E. Pieprneier, Jeffrey R. TI A comparison of near-concurrent measurements from the SSMIS and CoSMIR for some selected channels over the frequency range of 50-183 GHz SO IEEE TRANSACTIONS ON GEOSCIENCE AND REMOTE SENSING LA English DT Article DE calibration; microwave; radiometer; Special Sensor Microwave Imager/Sounder (SSMIS) ID ATMOSPHERIC WATER-VAPOR AB Ten underflights of the Special Sensor Microwave Imager/Sounder (SSMIS) with Conical Scanning Millimeter-wave Imaging Radiometer (CoSMIR) onboard the NASA ER-2 aircraft were conducted over the coastal region of California between March 2004 and March 2005. The measured brightness temperature (T-b) values from both sensors are collocated and compared at frequencies of 50.3, 52.8, 53.6, 91.655, 150,183.3 +/- 1, 183.3 +/- 3, and 183.3 +/- 6.6 GHz. The more transparent channels at 50.3, 91.655, and 150 GHz are strongly affected by the changes in surface emission and low-level liquid clouds. Thus, the average differences in T-b, values (delta T-b), measured by the two sensors, and their changes from flight to flight are difficult to assess. For the remaining opaque channels, using the CoSMIR measurements as reference, the lowest SSMIS Tb values occur when the SSMIS is completely under the Earth's shadow. As the satellite moves out of the Earth's shadow in the ascending passes, the SSMIS Tb values are found to gradually increase with more exposure to the sun. The magnitudes of these T-b changes are about 4-5 K for the three 183.3-GHz channels and about 2 K for the 52.8- and 53.6-GHz channels. C1 [Wang, James R.; Racette, Paul E.; Pieprneier, Jeffrey R.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Wang, JR (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. EM james.r.wang@nasa.gov NR 8 TC 7 Z9 7 U1 0 U2 1 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855 USA SN 0196-2892 J9 IEEE T GEOSCI REMOTE JI IEEE Trans. Geosci. Remote Sensing PD APR PY 2008 VL 46 IS 4 BP 923 EP 933 DI 10.1109/TGRS.2007.904038 PN 1 PG 11 WC Geochemistry & Geophysics; Engineering, Electrical & Electronic; Remote Sensing; Imaging Science & Photographic Technology SC Geochemistry & Geophysics; Engineering; Remote Sensing; Imaging Science & Photographic Technology GA 285YJ UT WOS:000254811800006 ER PT J AU Swadley, SD Poe, GA Bell, W Hong, Y Kunkee, DB McDermid, S Leblanc, T AF Swadley, Steven D. Poe, Gene A. Bell, William Hong, Ye Kunkee, David B. McDermid, Stuart Leblanc, Thierry TI Analysis and characterization of the SSMIS upper atmosphere sounding channel measurements SO IEEE TRANSACTIONS ON GEOSCIENCE AND REMOTE SENSING LA English DT Article DE calibration; Doppler frequency shift; microwave; polarized radiative transfer; radiometer; Special Sensor Microwave Imager/Sounder (SSMIS); Zeeman effect ID TEMPERATURE-MEASUREMENTS; OXYGEN; MESOSPHERE; FIELD; MODEL; PROPAGATION; FREQUENCIES; VALIDATION; SPECTRUM; MIDDLE AB Analyses and results of the radiometric calibration accuracy and measurement characteristics of the first Defense Meteorological Satellite Program (DMSP)'s Special Sensor Microwave Imager/Sounder (SSMIS) upper atmosphere sounding (IJAS) channels are presented herein. Launched on October 18, 2003, aboard the DMSP F-16 spacecraft in a sun-synchronous orbit, the SSMIS UAS channels provide the first operational measurements of microwave radiation emitted by the Earth's atmosphere at mesospheric altitudes. The analysis of the SSMIS radiometer absolute calibration and stability is based upon extensive comparisons with a fully polarimetric radiative transfer model (RTM) that solves for all four Stokes parameters using coincident atmospheric temperature profiles derived from collocated Rayleigh lidar observations merged with the European Centre for Medium-Range Weather Forecasting temperature analyses and climatological data sets. The resulting merged profiles provide a physically consistent temperature profile from the surface to 100 km, as needed by the RTMs. The results presented herein of the SSMIS instrument show that significant hardware and scientific technical challenges arise from microwave temperature sounding of the mesosphere. These include the following: 1) addressing the impact of large noise-equivalent temperature difference associated with narrow channel bandwidths; 2) achieving high channel center-frequency stability; 3) compensation of large spacecraft-induced Doppler shift; 4) better characterization of the Zeeman splitting of the oxygen absorption lines; 5) development of a fast polarimetric RTM; and 6) designing stable and accurate on-orbit radiometric calibration targets. Results to date show that the uncertainties of the calibration accuracy of the SSMIS UAS channels are consistent and in agreement with the limits derived for the SSMIS UAS channels and with the simulated radiances derived from the merged lidar profiles. C1 [Swadley, Steven D.] METOC Consulting, Monterey, CA 93943 USA. [Swadley, Steven D.; Poe, Gene A.] USN, Res Lab, Monterey, CA 93943 USA. [Bell, William] Satellite Radiance Assimilat Grp, Met Off, Exeter EX1 3PB, Devon, England. [Hong, Ye; Kunkee, David B.] Aerosp Corp, El Segundo, CA 90245 USA. [McDermid, Stuart; Leblanc, Thierry] CALTECH, Jet Prop Lab, Table Mt Facil, Wrightwood, CA 92397 USA. RP Swadley, SD (reprint author), METOC Consulting, Monterey, CA 93943 USA. EM steve.swadley@nrlmry.navy.mil NR 35 TC 14 Z9 14 U1 0 U2 6 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855 USA SN 0196-2892 J9 IEEE T GEOSCI REMOTE JI IEEE Trans. Geosci. Remote Sensing PD APR PY 2008 VL 46 IS 4 BP 962 EP 983 DI 10.1109/TGRS.2008.916980 PN 1 PG 22 WC Geochemistry & Geophysics; Engineering, Electrical & Electronic; Remote Sensing; Imaging Science & Photographic Technology SC Geochemistry & Geophysics; Engineering; Remote Sensing; Imaging Science & Photographic Technology GA 285YJ UT WOS:000254811800009 ER PT J AU Freeman, A AF Freeman, A. TI Response to "Corrections to 'Calibration of linearly polarized polarimetric SAR data subject to faraday rotation'" SO IEEE TRANSACTIONS ON GEOSCIENCE AND REMOTE SENSING LA English DT Letter DE cafibration; Faraday rotation; polarimetry; syntethic aperture radar (SAR) C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Freeman, A (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. NR 2 TC 2 Z9 2 U1 0 U2 3 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855 USA SN 0196-2892 J9 IEEE T GEOSCI REMOTE JI IEEE Trans. Geosci. Remote Sensing PD APR PY 2008 VL 46 IS 4 BP 1279 EP 1279 DI 10.1109/TGRS.2008.919875 PN 2 PG 1 WC Geochemistry & Geophysics; Engineering, Electrical & Electronic; Remote Sensing; Imaging Science & Photographic Technology SC Geochemistry & Geophysics; Engineering; Remote Sensing; Imaging Science & Photographic Technology GA 285YL UT WOS:000254812000022 ER PT J AU Schulze-Makuch, D Fairen, AG Davila, AF AF Schulze-Makuch, Dirk Fairen, Alberto G. Davila, Alfonso F. TI The case for life on Mars SO INTERNATIONAL JOURNAL OF ASTROBIOLOGY LA English DT Review DE Life; Mars; water; habitability; Viking; ALH84001; Panspermia ID MARTIAN METEORITE ALH84001; BACILLUS-SUBTILIS SPORES; GAS-EXCHANGE EXPERIMENT; LONG-TERM SURVIVAL; MAGNETOTACTIC BACTERIA; MAGNETITE CRYSTALS; NORTHERN PLAINS; MICROBIAL METHANOGENESIS; EXTREME ENVIRONMENTS; ATMOSPHERIC METHANE AB There have been several attempts to answer the question of whether there is. or has ever been. life oil Mars. The boldest attempt was the only ever life detection experiment conducted oil another planet : the Viking mission. The mission was a great Success, but it failed to provide I clear answer to the question of life Oil Mars. More than 30 years after the Viking mission our understanding of the history and evolution of Mars, has increased vastly to reveal,I wetter Martian past and the Occurrence of diverse environments that Could have Supported microbial life similar to that oil Earth for extended periods of time. The discovery of Terran extremophilic microorganisms. adapted to environments previously though to be Prohibitive for lifer has greatly expanded the limits of habitability in our Solar System, and has opened new avenues For the search of life oil Mars. Remnants of a possible early biosphere may be found in the Martian meteorite ALH84001. This claim is based oil I collection of facts and observations consistent with biogenic origins, but individual links in the collective chain of evidence remain controversial. Recent evidence for contemporary liquid water oil Mars and the detection of methane in the Martian atmosphere further enhance the case for life oil Mars. We argue that. given the cumulative evidence provided, life has and is likely to exist oil Mars, and we have already found evidence of it. However, to obtain a compelling certainty a new, mission is needed. one which is devoted to the detection of life oil mars. C1 [Schulze-Makuch, Dirk] Washington State Univ, Sch Earth & Environm Sci, Pullman, WA 99163 USA. [Fairen, Alberto G.; Davila, Alfonso F.] NASA, Ames Res Ctr, Space Sci & Astrobiol Div, Washington, DC 20546 USA. RP Schulze-Makuch, D (reprint author), Washington State Univ, Sch Earth & Environm Sci, Pullman, WA 99163 USA. EM dirksm@wsu.edu RI Davila, Alfonso/A-2198-2013; OI Davila, Alfonso/0000-0002-0977-9909; Schulze-Makuch, Dirk/0000-0002-1923-9746 NR 219 TC 18 Z9 18 U1 15 U2 58 PU CAMBRIDGE UNIV PRESS PI NEW YORK PA 32 AVENUE OF THE AMERICAS, NEW YORK, NY 10013-2473 USA SN 1473-5504 EI 1475-3006 J9 INT J ASTROBIOL JI Int. J. Astrobiol. PD APR PY 2008 VL 7 IS 2 BP 117 EP 141 DI 10.1017/S1473550408004175 PG 25 WC Astronomy & Astrophysics; Biology; Geosciences, Multidisciplinary SC Astronomy & Astrophysics; Life Sciences & Biomedicine - Other Topics; Geology GA 541AL UT WOS:000273382900003 ER PT J AU Coyne, JT Baldwin, CL Latorella, KA AF Coyne, Joseph T. Baldwin, Caffyl L. Latorella, Kara A. TI Pilot weather assessment: Implications for visual flight rules flight into instrument meteorological conditions SO INTERNATIONAL JOURNAL OF AVIATION PSYCHOLOGY LA English DT Article ID ADVERSE WEATHER; DECISIONS AB Visual flight rules flight into instrument meteorological conditions (IMC) account for over 10% of the fatalities in general aviation. Evidence suggests that pilots' assessments of weather conditions are related to their decision to continue. This study investigated pilots'ability to assess ceiling and visibility in a flight simulator. Assessment accuracy did not differ between instrument- and non-instrument-rated pilots for ceiling accuracy, but visibility accuracy was better for non-instrument-rated pilots. The data indicated pilots allowed their estimates of ceiling and visibility to influence each other. That is, pilots tended to judge a ceiling to be higher than it actually was when it was paired with a high visibility. This interaction may play a significant role in pilots' decisions to continue into IMC. C1 [Coyne, Joseph T.] USN, Res Lab, Washington, DC 20375 USA. [Baldwin, Caffyl L.] Old Dominion Univ, Norfolk, VA USA. [Latorella, Kara A.] NASA, Langley Res Ctr, Hampton, VA 23665 USA. RP Coyne, JT (reprint author), USN, Res Lab, Code 5511,4555 Overlook Ave SW, Washington, DC 20375 USA. EM coyne@itd.nrl.navy.mil NR 12 TC 2 Z9 2 U1 1 U2 2 PU TAYLOR & FRANCIS INC PI PHILADELPHIA PA 325 CHESTNUT ST, SUITE 800, PHILADELPHIA, PA 19106 USA SN 1050-8414 J9 INT J AVIAT PSYCHOL JI Int. J. Aviat. Psychol. PD APR-JUN PY 2008 VL 18 IS 2 BP 153 EP 166 DI 10.1080/10508410801926756 PG 14 WC Psychology, Applied SC Psychology GA 294NO UT WOS:000255413000002 ER PT J AU Huebner, LD Hall, RM Haynes, DA Pamadi, BN Taylor, TL Seaford, CM AF Huebner, Lawrence D. Hall, Robert M. Haynes, Davy A. Pamadi, Bandu N. Taylor, Terry L. Seaford, C. Mark TI Status, plans and initial results for Ares I Crew Launch Vehicle aerodynamics SO JBIS-JOURNAL OF THE BRITISH INTERPLANETARY SOCIETY LA English DT Article; Proceedings Paper CT 57th International Astronautical Congress CY OCT 02-06, 2006 CL Valencia, SPAIN DE Ares I Crew Launch Vehicle; aerodynamics; wind tunnel testing; computational fluid dynamics AB Following the completion of NASA's Exploration Systems Architecture Study in August 2004 for the NASA Exploration Systems Mission Directorate (ESMD), the Ares Projects Office at the NASA Marshall Space Flight Center was assigned project management responsibilities for the design and development of the first vehicle in the architecture, the Ares I Crew Launch Vehicle (CLV), which will be used to launch astronauts to low earth orbit and rendezvous with either the International Space Station or the ESMD's earth departure stage for lunar or other future missions beyond low Earth orbit. The primary elements of the Ares I CLV project are the first stage, the upper stage, the upper stage engine, and vehicle integration. Within vehicle integration is an effort in integrated design and analysis which is comprised of a number of technical disciplines needed to support vehicle design and development. One of the important disciplines throughout the life of the project is aerodynamics. This paper will present the status, plans, and initial results of Ares I CLV aerodynamics as the project was preparing for the Ares I CLV Systems Requirements Review. Following a discussion of the specific interactions with other technical panels and a status of the current activities, the plans for aerodynamic support of the Ares I CLV until the initial crewed flights will be presented. C1 [Huebner, Lawrence D.; Hall, Robert M.; Pamadi, Bandu N.] NASA, Langley Res Ctr, Hampton, VA 23681 USA. [Haynes, Davy A.; Taylor, Terry L.; Seaford, C. Mark] NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA. RP Huebner, LD (reprint author), NASA, Langley Res Ctr, Hampton, VA 23681 USA. EM Lawrence.D.Huebner@nasa.gov; Robert.M.Hall@nasa.gov; Davy.A.Haynes@nasa.gov; Bandu.N.Pamadi@nasa.gov; Terry.L.Taylor@nasa.gov; Dr.C.Seaford@nasa.gov NR 2 TC 2 Z9 2 U1 0 U2 0 PU BRITISH INTERPLANETARY SOC PI LONDON PA 27-29 S LAMBETH RD, LONDON SW8 1SZ, ENGLAND SN 0007-084X J9 JBIS-J BRIT INTERPLA JI JBIS-J. Br. Interplanet. Soc. PD APR PY 2008 VL 61 IS 4 BP 128 EP 138 PG 11 WC Engineering, Aerospace; Astronomy & Astrophysics; Geosciences, Multidisciplinary SC Engineering; Astronomy & Astrophysics; Geology GA 275AG UT WOS:000254043700003 ER PT J AU Jiang, HY Halverson, JB Simpson, J Zipser, EJ AF Jiang, Haiyan Halverson, Jeffrey B. Simpson, Joanne Zipser, Edward J. TI Hurricane "Rainfall Potential" derived from satellite observations aids overland rainfall prediction SO JOURNAL OF APPLIED METEOROLOGY AND CLIMATOLOGY LA English DT Article ID MICROWAVE SOUNDING UNIT; ATLANTIC TROPICAL CYCLONES; PRECIPITATION CHARACTERISTICS; GLOBAL PRECIPITATION; STORM RAINFALL; TRAP TECHNIQUE; PART II; ALGORITHMS; INTENSITY; LANDFALL AB The Tropical Rainfall Measuring Mission-based National Aeronautics and Space Administration Goddard Multisatellite Precipitation Analysis (MPA) product is used to quantify the rainfall distribution in tropical cyclones that made landfall in the United States during 1998-2004. A total of 37 tropical cyclones (TC) are examined, including 2680 three-hourly MPA precipitation observations. Rainfall distributions for overland and overocean observations are compared. It is found that the TC rainfall over ocean bears a strong relationship with the TC maximum wind, whereas the relationship for overland conditions is much weaker. The rainfall potential is defined by using the satellite-derived rain rate, the satellite-derived storm size, and the storm translation speed. This study examines the capability of the overocean rainfall potential to predict a storm's likelihood of producing heavy rain over land. High correlations between rain potentials before landfall and the maximum storm total rain over land are found using the dataset of the 37 landfalling TCs. Correlations are higher with the average rain potential on the day prior to landfall than with averages over any other time period. A TC overland rainfall index is introduced based on the rainfall potential study. This index can be used to predict the storm peak rainfall accumulation over land. Six landfalling storms during the 2005 Atlantic Ocean hurricane season are examined to verify the capability of using this index to forecast the maximum storm total rain over land in the United States. The range of the maximum storm overland rain forecast error for these six storms is between 2.5% and 24.8%. C1 [Jiang, Haiyan; Halverson, Jeffrey B.] Univ Maryland, Joint Ctr Earth Syst Technol, Baltimore, MD 21201 USA. [Jiang, Haiyan] NASA, Goddard Space Flight Ctr, Mesoscale Atmospher Proc Branch, Greenbelt, MD 20771 USA. [Simpson, Joanne] NASA, Goddard Space Flight Ctr, Atmospheres Lab, Greenbelt, MD 20771 USA. [Zipser, Edward J.] Univ Utah, Dept Meteorol, Salt Lake City, UT 84112 USA. RP Jiang, HY (reprint author), 135 S 1460 E,Rm 819 WBB, Salt Lake City, UT 84112 USA. EM h.jiang@utah.edu NR 35 TC 13 Z9 13 U1 0 U2 3 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 1558-8424 J9 J APPL METEOROL CLIM JI J. Appl. Meteorol. Climatol. PD APR PY 2008 VL 47 IS 4 BP 944 EP 959 DI 10.1175/2007JAMC1619.1 PG 16 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 302RG UT WOS:000255986400002 ER PT J AU Arguez, A Yu, P O'Brien, JJ AF Arguez, Anthony Yu, Peng O'Brien, James J. TI A new method for time series filtering near endpoints SO JOURNAL OF ATMOSPHERIC AND OCEANIC TECHNOLOGY LA English DT Article ID TEMPERATURES; OSCILLATION AB Time series filtering (e. g., smoothing) can be done in the spectral domain without loss of endpoints. However, filtering is commonly performed in the time domain using convolutions, resulting in lost points near the series endpoints. Multiple incarnations of a least squares minimization approach are developed that retain the endpoint intervals that are normally discarded due to filtering with convolutions in the time domain. The techniques minimize the errors between the predetermined frequency response function (FRF) - a fundamental property of all filters - of interior points with FRFs that are to be determined for each position in the endpoint zone. The least squares techniques are differentiated by their constraints: 1) unconstrained, 2) equal-mean constraint, and 3) an equal-variance constraint. The equal-mean constraint forces the new weights to sum up to the same value as the predetermined weights. The equal-variance constraint forces the new weights to be such that, after convolved with the input values, the expected time series variance is preserved. The three least squares methods are each tested under three separate filtering scenarios [involving Arctic Oscillation (AO), Madden-Julian oscillation (MJO), and El Nino-Southern Oscillation (ENSO) time series] and compared to each other as well as to the spectral filtering method - the standard of comparison. The results indicate that all four methods (including the spectral method) possess skill at determining suitable endpoints estimates. However, both the unconstrained and equal-mean schemes exhibit bias toward zero near the terminal ends due to problems with appropriating variance. The equal-variance method does not show evidence of this attribute and was never the worst performer. The equal-variance method showed great promise in the ENSO project involving a 5-month running mean filter, and performed at least on par with the other realistic methods for almost all time series positions in all three filtering scenarios. C1 [Arguez, Anthony] NOAA, NCDC, Asheville, NC 28801 USA. [Yu, Peng] CALTECH, Jet Prop Lab, Pasadena, CA USA. [O'Brien, James J.] Ctr Ocean Atmospher Predict Studies, Tallahassee, FL USA. RP Arguez, A (reprint author), NOAA, NCDC, CAB 514,151 Patton Ave, Asheville, NC 28801 USA. EM anthony.arguez@noaa.gov NR 13 TC 8 Z9 8 U1 1 U2 2 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 0739-0572 EI 1520-0426 J9 J ATMOS OCEAN TECH JI J. Atmos. Ocean. Technol. PD APR PY 2008 VL 25 IS 4 BP 534 EP 546 DI 10.1175/2007JTECHA924.1 PG 13 WC Engineering, Ocean; Meteorology & Atmospheric Sciences SC Engineering; Meteorology & Atmospheric Sciences GA 291CF UT WOS:000255169200003 ER PT J AU Su, WY Dutton, E Charlock, TP Wiscombe, W AF Su, Wenying Dutton, Ellsworth Charlock, Thomas P. Wiscombe, Warren TI Performance of commercial radiometers in very low temperature and pressure environments typical of polar regions and of the stratosphere: A laboratory study SO JOURNAL OF ATMOSPHERIC AND OCEANIC TECHNOLOGY LA English DT Article ID LONGWAVE IRRADIANCE UNCERTAINTY; THERMAL OFFSET; RADIATION; PYRGEOMETERS; CALIBRATION AB Characterizing the performance of ground-based commercial radiometers in cold and/or low-pressure environments is critical for developing accurate flux measurements in the polar regions and in the upper troposphere and stratosphere. Commercially available broadband radiometers have a stated operational temperature range of, typically, -20 degrees to +50 degrees C. Within this range, their temperature dependencies of sensitivities change less than 1%. But for deployments on high-altitude platforms or in polar regions, which can be much colder than -20 degrees C, information on temperature dependency of sensitivity is not always available. In this paper, the temperature dependencies of sensitivities of popular pyranometers and pyrgeometers manufactured by Kipp and Zonen were tested in a thermal-vacuum chamber. When their body temperature is lowered to -60 degrees C, pyranometer sensitivity drops by 4%-6% from the factory-default specification. Pyrgeometer sensitivity increases by 13% from the factory-default specification during a similar temperature change. When the chamber pressure is lowered from 830 to 6 hPa, the sensitivity decreases by about 2% for the pyranometer, and increases by about 2% for the pyrgeometer. Note that these temperature and pressure dependencies of sensitivities are specific for the instruments that were tested and should not be applied to others. These findings show that for measurements suitable for climate studies, it is crucial to characterize temperature and/or pressure effects on radiometer sensitivity for deployments on high-altitude platforms and in polar regions. C1 [Su, Wenying; Charlock, Thomas P.] NASA, Langley Res Ctr, Hampton, VA 23681 USA. [Su, Wenying] Sci Syst & Applicat Inc, Hampton, VA USA. [Dutton, Ellsworth] NOAA, Global Monitoring Div, Boulder, CO USA. [Wiscombe, Warren] NASA, Goddard Space Flight Ctr, Hampton, VA 23681 USA. RP Su, WY (reprint author), NASA, Langley Res Ctr, Mail Stop 420, Hampton, VA 23681 USA. EM wenying.su-1@nasa.gov RI Wiscombe, Warren/D-4665-2012 OI Wiscombe, Warren/0000-0001-6844-9849 NR 18 TC 3 Z9 3 U1 0 U2 2 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 0739-0572 J9 J ATMOS OCEAN TECH JI J. Atmos. Ocean. Technol. PD APR PY 2008 VL 25 IS 4 BP 558 EP 569 DI 10.1175/2007JTECHA1005.1 PG 12 WC Engineering, Ocean; Meteorology & Atmospheric Sciences SC Engineering; Meteorology & Atmospheric Sciences GA 291CF UT WOS:000255169200005 ER PT J AU Xu, KM Wong, T Wielicki, BA Parker, L AF Xu, Kuan-Man Wong, Takmeng Wielicki, Bruce A. Parker, Lindsay TI Statistical analyses of satellite cloud object data from CERES. Part IV: Boundary layer cloud objects during 1998 El Nino SO JOURNAL OF CLIMATE LA English DT Article ID MARINE STRATOCUMULUS CLOUDS; ANGULAR-DISTRIBUTION MODELS; RADIATIVE FLUX ESTIMATION; ENERGY SYSTEM INSTRUMENT; SURFACE OBSERVATIONS; GENERAL-CIRCULATION; STRATIFORM CLOUDS; LIQUID WATER; ISCCP; PACIFIC AB Three boundary layer cloud object types-overcast, stratocumulus, and cumulus-that occurred over the Pacific Ocean during January-August 1998 are identified from the Clouds and the Earth's Radiant Energy System (CERES) single scanner footprint data. Characteristics of each cloud object type matched with atmospheric states are examined for large regions in the tropics and subtropics and for different size categories. Stratocumulus cloud objects dominate the entire boundary layer cloud population in all regions and size categories. Overcast cloud objects, which have the largest average size, are more prevalent in the subtropics and near the coastal regions, while cumulus cloud objects are prevalent over the open oceans and the equatorial regions, particularly within the small-size categories. Cloud objects with equivalent diameters less than 75 km are excluded in the analysis. The differences between the tropical and subtropical statistical distributions of cloud properties are small for liquid water path (LWP), cloud optical depth, and top-of-the-atmosphere (TOA) albedo, but large for cloud-top temperature and outgoing longwave radiation (OLR), for each of the three cloud object types. The larger cloud objects have higher LWPs, cloud optical depths, TOA albedos, and OLRs, but lower SSTs and cloud-top heights for the stratocumulus and overcast types. Lower-tropospheric stability seems to be the primary factor for the differences in the distributions of cloud physical properties between the regions or between the size categories. Atmospheric dynamics also play a role in determining the differences in the distributions of cloud physical properties between the size categories, but not a significant role for those between the types or between the regions. The latter may be due to uncertainties in the matched vertical velocity data. When the three cloud object types are combined in small regions, lower-tropospheric stability determines the transition of boundary layer cloud types along a Pacific transect. The proportion of each type is the most important factor for diagnosing the combined cloud properties along this transect, such as LWP, cloud optical depth, and TOA albedo. Atmospheric dynamics also play complicated roles in determining the combined cloud properties along this transect. C1 [Xu, Kuan-Man; Wong, Takmeng; Wielicki, Bruce A.] NASA, Langley Res Ctr, Climate Sci Branch, Hampton, VA 23681 USA. [Parker, Lindsay] Sci Syst Applicat Inc, Hampton, VA USA. RP Xu, KM (reprint author), NASA, Langley Res Ctr, Climate Sci Branch, 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 NR 49 TC 19 Z9 19 U1 0 U2 3 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 0894-8755 J9 J CLIMATE JI J. Clim. PD APR 1 PY 2008 VL 21 IS 7 BP 1500 EP 1521 DI 10.1175/2007JCLI1710.1 PG 22 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 288RR UT WOS:000255004000004 ER PT J AU Hartley, TT Lorenzo, CF AF Hartley, Tom T. Lorenzo, Carl F. TI Application of Incomplete Gamma Functions to the Initialization of Fractional-Order Systems SO JOURNAL OF COMPUTATIONAL AND NONLINEAR DYNAMICS LA English DT Article CT ASME International Design Engineering Technical Conferences/Computers and Information in Engineering Conference CY SEP 04-07, 2007 CL Las Vegas, NV SP ASME, Design Engn Div, ASME, Comp & Informat Engn Div DE gamma function; fractional-order system initialization AB This paper reviews some properties of the gamma function, particularly the incomplete gamma function and its complement, as a function of the Laplace variable s. The utility of these functions in the solution of initialization problems in fractional-order system theory is demonstrated. Several specific differential equations are presented, and their initialization responses are found for a variety of initializations. Both the time-domain and Laplace-domain solutions are obtained and compared. The complementary incomplete gamma function is shown to be essential in finding the Laplace-domain solution of a fractional-order differential equation. C1 [Hartley, Tom T.] Univ Akron, Akron, OH 44325 USA. [Lorenzo, Carl F.] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. RP Hartley, TT (reprint author), Univ Akron, Akron, OH 44325 USA. EM thartley@uakron.edu; carl.f.lorenzo@nasa.gov NR 4 TC 4 Z9 4 U1 1 U2 2 PU ASME-AMER SOC MECHANICAL ENG PI NEW YORK PA THREE PARK AVE, NEW YORK, NY 10016-5990 USA SN 1555-1423 J9 J COMPUT NONLIN DYN JI J. Comput. Nonlinear Dyn. PD APR PY 2008 VL 3 IS 2 AR 021103 DI 10.1115/1.2833480 PG 6 WC Engineering, Mechanical; Mechanics SC Engineering; Mechanics GA 359QC UT WOS:000260002200004 ER PT J AU Lorenzo, CF Hartley, TT AF Lorenzo, Carl F. Hartley, Tom T. TI Initialization of Fractional-Order Operators and Fractional Differential Equations SO JOURNAL OF COMPUTATIONAL AND NONLINEAR DYNAMICS LA English DT Article CT ASME International Design Engineering Technical Conferences/Computers and Information in Engineering Conference CY SEP 04-07, 2007 CL Las Vegas, NV SP ASME, Design Engn Div, ASME, Comp & Informat Engn Div ID SYSTEMS AB It has been known that the initialization of fractional operators requires time-varying functions, a complicating factor; This paper simplifies the process of initialization of fractional differential equations by deriving Laplace transforms for the initialized fractional integral and derivative that generalize those for the integer-order operators. The new transforms unify the initialization of systems of fractional and ordinary differential equations. The paper provides background on past work in the area and determines the Laplace transforms for the initialized fractional integral and fractional derivatives of any (real) order. An application provides insight and demonstrates the theory. C1 [Lorenzo, Carl F.] NASA, Glenn Res Ctr, Div Instrumentat & Controls, Cleveland, OH 44135 USA. [Hartley, Tom T.] Univ Akron, Dept Elect & Comp Engn, Akron, OH 44325 USA. RP Lorenzo, CF (reprint author), NASA, Glenn Res Ctr, Div Instrumentat & Controls, Cleveland, OH 44135 USA. NR 13 TC 18 Z9 18 U1 1 U2 6 PU ASME-AMER SOC MECHANICAL ENG PI NEW YORK PA THREE PARK AVE, NEW YORK, NY 10016-5990 USA SN 1555-1423 J9 J COMPUT NONLIN DYN JI J. Comput. Nonlinear Dyn. PD APR PY 2008 VL 3 IS 2 AR 021101 DI 10.1115/1.2833585 PG 9 WC Engineering, Mechanical; Mechanics SC Engineering; Mechanics GA 359QC UT WOS:000260002200002 ER PT J AU Nourgaliev, RR Liou, MS Theofanous, TG AF Nourgaliev, R. R. Liou, M. -S. Theofanous, T. G. TI Numerical prediction of interfacial instabilities: Sharp interface method (SIM) SO JOURNAL OF COMPUTATIONAL PHYSICS LA English DT Article DE interfacial instability; interfacial flows; gas-liquid interfaces; sharp-interface treatment; viscous Kelvin-Helmholtz instability; Yih instability; Rayleigh-Taylor instability; instability-seeding in numerical simulations ID RAYLEIGH-TAYLOR INSTABILITY; INCOMPRESSIBLE 2-PHASE FLOWS; CHARACTERIZED VISCOELASTIC FLUIDS; NAVIER-STOKES EQUATIONS; DRIVEN CHANNEL FLOW; ADAPTIVE LEVEL SET; MULTIPHASE FLOW; SURFACE-TENSION; FRONT-TRACKING; LINEAR-STABILITY AB We introduce a sharp interface method (SIM) for the direct numerical simulation of unstable fluid-fluid interfaces. The method is based on the level set approach and the structured adaptive mesh refinement technology, endowed with a corridor of irregular, cut-cell grids that resolve the interfacial region to third-order spatial accuracy. Key in that regard are avoidance of numerical mixing, and a least-squares interpolation method that is supported by irregular datasets distinctly on each side of the interface. Results on test problems show our method to be free of the spurious current problem of the continuous surface force method and to converge, on grid refinement, at near-theoretical rates. Simulations of unstable Rayleigh-Taylor and viscous Kelvin-Helmholtz flows are found to converge at near-theoretical rates to the exact results over a wide range of conditions. Further, we show predictions of neutral-stability maps of the viscous Kelvin-Helmholtz flows (Yih instability), as well as self-selection of the most unstable wave-number in multimode simulations of Rayleigh-Taylor instability. All these results were obtained with a simple seeding of random infinitesimal disturbances of interface-shape, as opposed to seeding by a complete eigenmode. For other than elementary flows the latter would normally not be available, and extremely difficult to obtain if at all. Sample comparisons with our code adapted to mimic typical diffuse interface treatments were not satisfactory for shear-dominated flows. On the other hand the sharp dynamics of our method would appear to be compatible and possibly advantageous to any interfacial flow algorithm in which the interface is represented as a discrete Heaviside function. Published by Elsevier Inc. C1 [Nourgaliev, R. R.; Theofanous, T. G.] Univ Calif Santa Barbara, Ctr Risk Studies & Safety, Santa Barbara, CA 93106 USA. [Liou, M. -S.] NASA, Glenn Res Ctr, Aeroprop Div, Cleveland, OH USA. RP Nourgaliev, RR (reprint author), Idaho Natl Lab, Idaho Falls, ID 83415 USA. EM robert.nourgaliev@inl.gov; meng-sing.liou@grc.nasa.gov; theo@engr.ucsb.edu NR 74 TC 20 Z9 21 U1 0 U2 15 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0021-9991 J9 J COMPUT PHYS JI J. Comput. Phys. PD APR 1 PY 2008 VL 227 IS 8 BP 3940 EP 3970 DI 10.1016/j.jcp.2007.12.008 PG 31 WC Computer Science, Interdisciplinary Applications; Physics, Mathematical SC Computer Science; Physics GA 288BG UT WOS:000254960600011 ER PT J AU Trunek, AJ Neudeck, PG Matocha, K Dunne, G AF Trunek, Andrew J. Neudeck, Philip G. Matocha, Kevin Dunne, Greg TI Increased nitrogen doping of thin lateral SiC cantilevers SO JOURNAL OF CRYSTAL GROWTH LA English DT Article; Proceedings Paper CT 15th International Conference on Crystal Growth CY AUG 12-17, 2007 CL Salt Lake City, UT SP ACCG DE doping; cantilevers; chemical vapor deposition; mesas; silicon carbide; MOS capacitors ID EPITAXIAL-GROWTH; SURFACES; MESAS AB We report on a recently-observed difference in nitrogen doping during the growth of homoepitaxial films grown on on-axis 4H-SiC (SiC-silicon carbide) substrates patterned with arrays of mesas. In particular, the doping of webbed cantilevered regions that grew laterally from the tops of mesas free of axial screw dislocations was observed to be significantly greater than solid mesas with screw dislocations that grew vertically along the [0001] c-axis. (c) 2007 Elsevier B.V. All rights reserved. C1 [Trunek, Andrew J.] NASA Glenn, OAI, Cleveland, OH 44135 USA. [Neudeck, Philip G.] NASA, Glenn Res Ctr, Ohio Aerosp Inst, Cleveland, OH 44135 USA. [Matocha, Kevin; Dunne, Greg] GE Global Res, Niskayuna, NY 12309 USA. RP Trunek, AJ (reprint author), NASA Glenn, OAI, 21000 Brookpk Rd,MS 77-1, Cleveland, OH 44135 USA. EM Andrew.J.Trunek@grc.nasa.gov NR 12 TC 0 Z9 0 U1 0 U2 1 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0022-0248 J9 J CRYST GROWTH JI J. Cryst. Growth PD APR PY 2008 VL 310 IS 7-9 SI SI BP 1794 EP 1798 DI 10.1016/j.jcrysgro.2007.11.029 PG 5 WC Crystallography; Materials Science, Multidisciplinary; Physics, Applied SC Crystallography; Materials Science; Physics GA 300RP UT WOS:000255843200090 ER PT J AU Gubinyi, Z Batur, C Sayir, A Dynys, F AF Gubinyi, Z. Batur, C. Sayir, A. Dynys, F. TI Electrical properties of PZT piezoelectric ceramic at high temperatures SO JOURNAL OF ELECTROCERAMICS LA English DT Article DE high temperature PZT piezoceramic; changes in electrical and mechanical properties with respect to temperature ID SINGLE-CRYSTALS; THERMODYNAMIC THEORY; PHASE-TRANSITIONS AB Advanced aeronautic and space structures need active components that can function at high frequencies and temperatures. Piezoelectric materials can provide frequency response but their use at elevated temperatures is limited. The reason for the lack of insertion of piezoelectric for high temperature active component and sensors are two fold. First, the database of piezoelectric properties that describe the piezoelectric constants is lacking for high temperatures engineering applications. Most studies measure the dielectric constants to determine the Curie temperature but do not provide piezoelectric coefficients as a function of temperature. Second, piezoelectric materials with Curie temperature (T(C)) exceeding 500 degrees C are sought for aeronautics and aerospace applications. This investigation describes a measurement system that captures the impedance dependence upon temperature for piezoelectric materials. Commercially available lead zirconate titanate (PZT) was studied as to determine the piezoelectric activity to define the operating envelope with respect to temperature. The elastic properties (c(ijkl)(E)), piezoelectric coefficients (e(ik)(S)), dielectric properties (epsilon(S)(ik)), and electro-mechanical coupling factors were determined as a function of temperature. The coupling factor k(33) was found to be relatively constant to 200 degrees C and exhibit slight temperature dependence above 200 degrees C. The temperature sensitivity for both piezoelectric coefficient and electromechanical coupling factor were very small; the slopes Delta d(31)(T)/d(31)(T) and k(33)/k(33) were found to be 0.01 and (-0.07) respectively in the range of 120 to 200 degrees C. This measurement technique will populate databases that describe the piezoelectric properties of commercially available PZT piezoelectric materials. It can also facilitate the assessment of new piezoelectric materials that are currently being developed for higher temperature applications. C1 [Gubinyi, Z.; Batur, C.] Univ Akron, Dept Mech Engn, Akron, OH 44325 USA. [Sayir, A.; Dynys, F.] NASA Glenn Res Ctr, Cleveland, OH USA. RP Batur, C (reprint author), Univ Akron, Dept Mech Engn, Akron, OH 44325 USA. EM batur@uakron.edu NR 27 TC 20 Z9 20 U1 1 U2 26 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 1385-3449 J9 J ELECTROCERAM JI J. Electroceram. PD APR PY 2008 VL 20 IS 2 BP 95 EP 105 DI 10.1007/s10832-007-9364-3 PG 11 WC Materials Science, Ceramics SC Materials Science GA 259DX UT WOS:000252920400005 ER PT J AU De Witt, JK Hagan, RD Cromwell, RL AF De Witt, John K. Hagan, R. Donald Cromwell, Ronita L. TI The effect of increasing inertia upon vertical ground reaction forces and temporal kinematics during locomotion SO JOURNAL OF EXPERIMENTAL BIOLOGY LA English DT Article DE biomechanics; locomotion; ground reaction force; inertia; gravity; weight; mass; human ID SIMULATED REDUCED-GRAVITY; BODY-WEIGHT SUPPORT; CENTER-OF-MASS; HUMAN WALKING; METABOLIC COST; MECHANICS; PARAMETERS; ENERGETICS; INSIGHTS; BONE AB The addition of inertia to exercising astronauts could increase ground reaction forces and potentially provide a greater health benefit. However, conflicting results have been reported regarding the adaptations to additional mass (inertia) without additional net weight (gravitational force) during locomotion. We examined the effect of increasing inertia while maintaining net gravitational force on vertical ground reaction forces and temporal kinematics during walking and running. Vertical ground reaction force was measured for 10 healthy adults (five male/five female) during walking (1.34 m s(-1)) and running (3.13 m s(-1)) using a force-measuring treadmill. Subjects completed locomotion at normal weight and mass and at 10, 20, 30 and 40% of added inertial force. The added gravitational force was relieved with overhead suspension, so that the net force between the subject and treadmill at rest remained equal to 100% body weight. Ground reaction forces were affected by the added inertial force, but not to the magnitude predicted by the increase in mass, suggesting that adaptations in motion occurred. Vertical ground reaction force production and adaptations in gait temporal kinematics were different between walking and running. Peak vertical impact forces and loading rates increased with increased inertia during walking, and decreased during running. As inertia increased, peak vertical propulsive forces decreased during walking and did not change during running. Stride time increased during walking and running, and contact time increased during running. The increased inertial forces were utilized independently from gravitational forces by the motor control system when determining coordination strategies. C1 [De Witt, John K.] Wyles Life Sci Grp, Houston, TX 77058 USA. [Hagan, R. Donald] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. [Cromwell, Ronita L.] Univ Texas Galveston, Med Branch, Dept Phys Therapy, Galveston, TX USA. RP De Witt, JK (reprint author), Wyles Life Sci Grp, Houston, TX 77058 USA. EM john.k.dewitt@nasa.gov NR 25 TC 17 Z9 17 U1 0 U2 3 PU COMPANY OF BIOLOGISTS LTD PI CAMBRIDGE PA BIDDER BUILDING CAMBRIDGE COMMERCIAL PARK COWLEY RD, CAMBRIDGE CB4 4DL, CAMBS, ENGLAND SN 0022-0949 J9 J EXP BIOL JI J. Exp. Biol. PD APR PY 2008 VL 211 IS 7 BP 1087 EP 1092 DI 10.1242/jeb.012443 PG 6 WC Biology SC Life Sciences & Biomedicine - Other Topics GA 280YS UT WOS:000254463300015 PM 18344482 ER PT J AU Baldwin, RE Miller, TW Brodeur, RD Jacobson, KC AF Baldwin, R. E. Miller, T. W. Brodeur, R. D. Jacobson, K. C. TI Expanding the foraging history of juvenile Pacific salmon: combining stomach-content and macroparasite-community analyses for studying marine diets SO JOURNAL OF FISH BIOLOGY LA English DT Article DE food transmitted parasites; ocean ecology; salmon ID NORTHERN CALIFORNIA CURRENT; ONCORHYNCHUS-KISUTCH; COHO SALMON; LECITHASTER-GIBBOSUS; FEEDING CHRONOLOGY; LIFE-HISTORY; FOOD-HABITS; PARASITES; FISH; CHINOOK AB Stomach contents and macroparasites were examined from the same fishes collected off Oregon and California in June and August of 2000 and 2002 to provide a more comprehensive description of the diet of juvenile Chinook salmon Oncorhynchus tshawytscha and coho salmon Oncorhynchus kisutch during their first few months at sea. Temporal and spatial similarities of the two data sets were assessed using multivariate analyses. Both stomach contents and macroparasite communities indicated that fishes, euphausiids and hyperiid amphipods were consumed by both salmonid species, although their relative contribution to each species diet was highly variable. In June, the greater abundances of parasite species in Chinook salmon compared to coho salmon suggested that Chinook salmon consumed more infected intermediate hosts (crustaceans or larval fishes) shortly after ocean entry (April and May). Although the macroparasite analysis lacked the specificity of stomach analysis in identifying prey, macroparasites can provide a longer term history of feeding and diet information for fishes with empty stomachs. (c) 2008 The Authors Journal compilation (c) 2008 The Fisheries Society of the British Isles. C1 [Baldwin, R. E.; Miller, T. W.] Oregon State Univ, Hatfield Marine Sci Ctr, Cooperat Inst Marine Resources Studies, Newport, OR 97365 USA. [Brodeur, R. D.; Jacobson, K. C.] NOAA, Natl Marine Fisheries Serv, Northwest Fisheries Sci Ctr, Newport, OR 97365 USA. RP Baldwin, RE (reprint author), Oregon State Univ, Hatfield Marine Sci Ctr, Cooperat Inst Marine Resources Studies, Newport, OR 97365 USA. EM rebecca.baldwin@oregonstate.edu NR 50 TC 13 Z9 14 U1 0 U2 17 PU BLACKWELL PUBLISHING PI OXFORD PA 9600 GARSINGTON RD, OXFORD OX4 2DQ, OXON, ENGLAND SN 0022-1112 J9 J FISH BIOL JI J. Fish Biol. PD APR PY 2008 VL 72 IS 6 BP 1268 EP 1294 DI 10.1111/j.1095-8649.2007.01792.x PG 27 WC Fisheries; Marine & Freshwater Biology SC Fisheries; Marine & Freshwater Biology GA 285XJ UT WOS:000254809200003 ER PT J AU Choi, YH Vay, SA Vadrevu, KP Soja, AJ Woo, JH Nolf, SR Sachse, GW Diskin, GS Blake, DR Blake, NJ Singh, HB Avery, MA Fried, A Pfister, L Fuelberg, HE AF Choi, Yonghoon Vay, Stephanie A. Vadrevu, Krishna P. Soja, Amber J. Woo, Jung-Hun Nolf, Scott R. Sachse, Glen W. Diskin, Glenn S. Blake, Donald R. Blake, Nicola J. Singh, Hanwant B. Avery, Melody A. Fried, Alan Pfister, Leonhard Fuelberg, Henry E. TI Characteristics of the atmospheric CO2 signal as observed over the conterminous United States during INTEX-NA SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Review ID TRACE GAS-TRANSPORT; CARBON-DIOXIDE; NORTH-AMERICA; NITROGEN DEPOSITION; ASIAN EMISSIONS; SULFUR-DIOXIDE; ATLANTIC-OCEAN; AIR-POLLUTANTS; BOREAL FORESTS; PACIFIC AB High resolution in situ measurements of atmospheric CO2 were made from the NASA DC-8 aircraft during the Intercontinental Chemical Transport Experiment-North America (INTEX-NA) campaign, part of the wider International Consortium for Atmospheric Research on Transport and Transformation (ICARTT). During the summer of 2004, eighteen flights comprising 160 h of measurements were conducted within a region bounded by 27 to 53 degrees N and 36 to 139 degrees W over an altitude range of 0.15 to 12 km. These large-scale surveys provided the opportunity to examine the characteristics of the atmospheric CO2 signal over sparsely sampled areas of North America and adjacent ocean basins. The observations showed a high degree of variability (<= 18%) due to the myriad source and sink processes influencing the air masses intercepted over the INTEX-NA sampling domain. Surface fluxes had strong effects on continental scale concentration gradients. Clear signatures of CO2 uptake were seen east of the Mississippi River, notably a persistent CO2 deficit in the lowest 2-3 km. When combining the airborne CO2 measurements with LANDSAT and MODIS data products, the lowest CO2 mixing ratios observed during the campaign (337 ppm) were tied to mid-continental agricultural fields planted in corn and soybeans. We used simultaneous measurements of CO, O-3, C2Cl4, C2H6, C2H2 and other unique chemical tracers to differentiate air mass types. Coupling these distinct air mass chemical signatures with transport history permitted identification of convection, stratosphere-troposphere exchange, long-range transport from Eastern Asia, boreal wildfires, and continental outflow as competing processes at multiple scales influencing the observed concentrations. Our results suggest these are important factors contributing to the large-scale distribution in CO2 mixing ratios thus these observations offer new constraints in the computation of the North American carbon budget. C1 [Choi, Yonghoon; Soja, Amber J.] NIA, NASA, Langley Res Ctr, Hampton, VA 23666 USA. [Woo, Jung-Hun] Konkuk Univ, Dept Adv Technol Fus, Seoul, South Korea. [Vadrevu, Krishna P.] Ohio State Univ, Ohio Agr Res & Dev Ctr, Agroecosyst Management Program, Wooster, OH 44691 USA. [Nolf, Scott R.] Comp Sci Corp, Hampton, VA USA. [Blake, Donald R.; Blake, Nicola J.] Univ Calif Irvine, Dept Chem, Irvine, CA 92717 USA. [Singh, Hanwant B.; Pfister, Leonhard] Natl Ctr Atmospher Res, Boulder, CO 80307 USA. [Fuelberg, Henry E.] Florida State Univ, Dept Meteorol, Tallahassee, FL 32306 USA. RP Choi, YH (reprint author), NIA, NASA, Langley Res Ctr, 100 Explorat Way, Hampton, VA 23666 USA. EM ychoi@nianet.org OI Vadrevu, Krishna/0000-0003-4407-5605 NR 106 TC 19 Z9 19 U1 2 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 APR 1 PY 2008 VL 113 IS D7 AR D07301 DI 10.1029/2007JD008899 PG 16 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 284OY UT WOS:000254716900001 ER PT J AU Gasso, S AF Gasso, Santiago TI Satellite observations of the impact of weak volcanic activity on marine clouds SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID SOUTH SANDWICH ISLANDS; SHIP TRACKS; SIZE DISTRIBUTIONS; OCEAN PRODUCTIVITY; STRATIFORM CLOUDS; SULFUR EMISSIONS; WATER-VAPOR; LEE WAVES; CLIMATE; AEROSOL AB Because emissions from weak volcanic eruptions tend to remain in the low troposphere, they may have a significant radiative impact through the indirect effect on clouds. However, this type of volcanic activity is underreported and its global impact has been assessed only by model simulations constrained with very limited observations. First observations of the impact of high- latitude active volcanoes on marine boundary layer clouds are reported here. These observations were made using a combination of standard derived products and visible images from the MODIS, AMSR- E and GOES detectors. Two distinctive effects are identified. When there is an existing boundary layer cloud deck, an increase in cloud brightness and a decrease in both cloud effective radius and liquid water content were observed immediately downwind of the volcanoes. The visible appearance of these "volcano tracks'' resembles the effect of man-made ship tracks. When synoptic conditions favor low cloudiness, the volcano plume ( or volcano cloud) increases significantly the cloud cover downwind. The volcano cloud can extend for hundreds of kilometers until mixing with background clouds. Unlike violent eruptions, the volcano clouds reported here ( the Aleutian Islands in the North Pacific and the South Sandwich Islands in the South Atlantic) have retrieved microphysical properties similar to those observed in ship tracks. However, when comparing the volcano clouds from these two regions, liquid water content can decrease, increase or remain unchanged with respect to nearby unperturbed clouds. These differences suggest that composition at the source, type of eruption and meteorological conditions influence the evolution of the cloud. C1 [Gasso, Santiago] Univ Maryland, Goddard Earth Sci & Technol Ctr, Baltimore, MD 21201 USA. RP Gasso, S (reprint author), NASA, Goddard Space Flight Ctr, Code 613-2, Greenbelt, MD 20771 USA. EM santiago@climate.gsfc.nasa.gov RI Gasso, Santiago/H-9571-2014 OI Gasso, Santiago/0000-0002-6872-0018 NR 83 TC 34 Z9 34 U1 0 U2 4 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD APR 1 PY 2008 VL 113 IS D14 AR D14S19 DI 10.1029/2007JD009106 PG 14 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 284PB UT WOS:000254717200001 ER PT J AU Leuschen, CJ Swift, RN Comiso, JC Raney, RK Chapman, RD Krabill, WB Sonntag, JG AF Leuschen, Carlton J. Swift, Robert N. Comiso, Josefino C. Raney, R. Keith Chapman, Rickey D. Krabill, William B. Sonntag, John G. TI Combination of laser and radar altimeter height measurements to estimate snow depth during the 2004 Antarctic AMSR-E Sea Ice field campaign SO JOURNAL OF GEOPHYSICAL RESEARCH-OCEANS LA English DT Article ID ARCTIC-OCEAN; VARIABILITY; ROUGHNESS; SHEETS; COVER AB Among the most important parameters needed to evaluate the present and future state of Antarctic sea ice cover is the ice thickness. The retrieval of ice thickness using remote sensing techniques has been hampered by the absence of a capability to remotely measure snow thickness covering the sea ice. Data sets collected with Johns Hopkins Applied Physics Laboratory's Delay-Doppler Phase Monopulse (D2P) radar and NASA's Airborne Topographic Mapper (ATM) scanning lidar during NASA's Antarctic AMSR-E Sea Ice field campaign over the Bellingshausen Sea are used to demonstrate the potential of a remote-sensing technique for retrieval of snow cover thickness from an airborne platform. The technique takes advantage of the fact that the radar is most sensitive to the snow-ice interface while the lidar responds to the highly optically reflective snow surface. The difference between the radar- and laser-determined surfaces yields an estimate of snow thickness that appears to be reasonably consistent with expected values. The technique requires careful registration of the instrument footprints. Because there was no absolute range calibration of the lidar due to predeployment scheduling difficulties, the vertical offset between the instruments was resolved by determining the difference between measurements over leads. Elsewhere over sea ice the radar-defined surface is generally below the laser-defined surface consistent with the radar defining the snow-ice interface. Over a relatively small portion of the data, we observed opposite relationship between the sensor-defined surfaces for which we discuss a plausible physical explanation. C1 [Leuschen, Carlton J.] Univ Kansas, Ctr Remote Sensing Ice Sheets, Lawrence, KS 66045 USA. [Swift, Robert N.; Sonntag, John G.] NASA, Goddard Space Flight Ctr, Observat Sci Branch, Wallops Isl, VA 23337 USA. [Comiso, Josefino C.] NASA, Goddard Space Flight Ctr, Cryospher Sci Branch, Greenbelt, MD 20771 USA. [Raney, R. Keith; Chapman, Rickey D.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD USA. RP Leuschen, CJ (reprint author), Univ Kansas, Ctr Remote Sensing Ice Sheets, 2335 Irving Hill Rd, Lawrence, KS 66045 USA. EM leuschen@eecs.ku.edu NR 31 TC 15 Z9 15 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 APR 1 PY 2008 VL 113 IS C4 AR C04S90 DI 10.1029/2007JC004285 PG 10 WC Oceanography SC Oceanography GA 284PH UT WOS:000254717800001 ER PT J AU Whitten, RC Borucki, WJ O'Brien, K Tripathi, SN AF Whitten, R. C. Borucki, W. J. O'Brien, K. Tripathi, S. N. TI Predictions of the electrical conductivity and charging of the cloud particles in Jupiter's atmosphere SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Article ID TRANSFER CROSS-SECTIONS; COSMIC-RAY IONIZATION; LOW ENERGIES; DENSITY; IONS; RECOMBINATION; STRATOSPHERE; MOBILITIES; AEROSOLS; DESCENT AB The electrical conductivity and electrical charge on cloud particles ( composed of ammonia, ammonium hydrosulfide, and water) in the atmosphere of Jupiter are computed for pressures between 5.5 and 0.1 bars. The source of ionization is galactic cosmic rays ( GCR). The distribution of charge among the various reservoirs is a function of altitude and the total area of the aerosol particles. For pressures below 4 bars, the electrons are scavenged efficiently by the cloud particles, decreasing the electron- ion recombination rate and resulting in increased positive ion abundance over that in the absence of the particles. For the upper regions of each cloud layer, the area of the aerosols and the large diffusion rate of the electrons cause most aerosol particles to be negatively charged. Near the bases of the cloud layers, the larger total area of the aerosols causes most of the charge, positive and negative, to reside on particles. Where clouds are present, the reduction of the electron conductivity ranges from a factor of 30 at 0.1 bar to 10 4 at 4 bars. At pressures near 1 bar and 4 bars, the positive ion conductivity increases by a factor of 10 over that expected for the clear atmosphere. A parametric study of negative ions shows that they are likely to be insignificant. For altitudes below the 0.3- bar level the predicted positive and negative conductivities are well below the detection limit of the relaxation and mutual impedance instruments such as those employed on the Huygens entry probe. C1 [Whitten, R. C.] SETI Inst, Mountain View, CA 94043 USA. [Borucki, W. J.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [O'Brien, K.] No Arizona Univ, Dept Phys & Astron, Flagstaff, AZ 86011 USA. [Tripathi, S. N.] Indian Inst Technol, Kanpur 208016, Uttar Pradesh, India. RP Whitten, RC (reprint author), SETI Inst, 515 N Whisman Rd, Mountain View, CA 94043 USA. EM rwhitten@pacbell.net RI Tripathi, Sachchida/J-4840-2016 NR 39 TC 10 Z9 10 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-PLANET JI J. Geophys. Res.-Planets PD APR 1 PY 2008 VL 113 IS E4 AR E04001 DI 10.1029/2007JE002975 PG 11 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 284PK UT WOS:000254718100001 ER PT J AU Kenyon, M Day, PK Bradford, CM Bock, JJ Leduc, HG AF Kenyon, M. Day, P. K. Bradford, C. M. Bock, J. J. Leduc, H. G. TI Electrical properties of background-limited membrane-isolation transition-edge sensing bolometers for Far-IR/Submillimeter direct-detection spectroscopy SO JOURNAL OF LOW TEMPERATURE PHYSICS LA English DT Article; Proceedings Paper CT 12th International Workshop on Low Temperature Detectors CY JUL 22-27, 2007 CL Paris, FRANCE DE transition-edge sensor; far-IR spectrometer; submillimeter spectrometer; Si(3)N4 AB We built and measured the electrical properties of membrane-isolation transition-edge sensing bolometers (TESs) suitable for background-limited far-IR/submillimeter direct-detection spectroscopy. Each TES consists of a Mo/Au bilayer patterned onto a suspended, thermally isolated absorber that is connected to the substrate through four Si (x) N (y) beams deposited by low pressure chemical vapor deposition (LPCVD). We fabricated TESs with straight and meander support beams. The dimensions of the meander (straight) support beams are 700 mu m (700 mu m) long by 0.25 mu m (0.5 mu m) thick by 0.35 mu m (0.5 mu m) wide. We measured I-V characteristics for these TESs and determined that the thermal conductance G equals 72 fW/K (straight) and 19 fW/K (meander) for our best devices. The thermal conductance exhibits a T-1/2 dependence with temperature which is evidence of effective elastic scattering of the acoustic phonon modes. The transition temperatures T-c for the same TESs are T-c =137 mK (straight) and T-c =71 mK (meander). If we assume the TESs are temperature-fluctuation noise limited, then the derived noise equivalent power (NEP) equals 1.9x10(-19) W/Hz(1/2) (straight) and 6.1x10(-20) W/Hz(1/2) (meander), using our measured values for G and T (c) . The meander-beam TES has a derived NEP that is close to two orders of magnitude lower than the state-of-the-art. Finally, we measured an effective time constant tau of about 300 ms (straight) and 400 ms (meander) using electrical and optical pulses. These values for the NEP and tau for the meander-beam TES meet the requirements for the Background-Limited far-IR/Submillimeter Spectrograph (BLISS), a proposed NASA instrument. C1 [Kenyon, M.; Day, P. K.; Bradford, C. M.; Bock, J. J.; Leduc, H. G.] Jet Propuls Lab, Pasadena, CA 91109 USA. RP Kenyon, M (reprint author), Jet Propuls Lab, Pasadena, CA 91109 USA. EM matthew.e.kenyon@jpl.nasa.gov NR 14 TC 15 Z9 15 U1 0 U2 4 PU SPRINGER/PLENUM PUBLISHERS PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0022-2291 J9 J LOW TEMP PHYS JI J. Low Temp. Phys. PD APR PY 2008 VL 151 IS 1-2 BP 112 EP 118 DI 10.1007/s10909-007-9630-4 PG 7 WC Physics, Applied; Physics, Condensed Matter SC Physics GA 270CP UT WOS:000253697900016 ER PT J AU Bonetti, JA Day, P Kenyon, M Turner, A Leduc, HG Kuo, CL Bock, JJ AF Bonetti, J. A. Day, P. Kenyon, M. Turner, A. LeDuc, H. G. Kuo, C. L. Bock, J. J. TI Electrical and thermal characterization of membrane-isolated, antenna-coupled, TES bolometers for the SPIDER experiment SO JOURNAL OF LOW TEMPERATURE PHYSICS LA English DT Article; Proceedings Paper CT 12th International Workshop on Low Temperature Detectors CY JUL 22-27, 2007 CL Paris, FRANCE DE TES bolometers; cosmology; CMB; cosmic microwave background; polarization ID ELECTROTHERMAL FEEDBACK AB We have fabricated and measured the thermal and DC electrical properties of transition-edge sensing (TES) bolometers to be employed on the SPIDER experiment, a balloon-based observatory for studying the polarization of the cosmic microwave background (CMB). The bolometers consist of Al and Ti thermistors in series and a termination resistor which couples to an on-chip, polarization sensitive, 150 GHz slot-array antenna through a superconducting microstrip transmission line. Several important parameters were measured. Transition temperature measurements were performed by measuring the Johnson noise in the Ti thermistor. Current-voltage characteristic measurements were performed at various temperatures allowing for the deduction of the thermal conductance and the temperature coefficient of resistance. Electrical noise equivalent power was measured to sub-Hertz frequencies. Finally, the time constant of the bolometers was measured within the Al and Ti transitions where electrothermal feedback speeds up the bolometer response compared with the natural time constant measured just above the Ti transition temperature. The results of these measurements are within the design specifications for SPIDER. C1 [Bonetti, J. A.; Day, P.; Kenyon, M.; Turner, A.; LeDuc, H. G.; Kuo, C. L.; Bock, J. J.] CALTECH, Jet Propuls Lab, Pasadena, CA 91109 USA. RP Bonetti, JA (reprint author), CALTECH, Jet Propuls Lab, Pasadena, CA 91109 USA. EM joseph.bonetti@jpl.nasa.gov NR 2 TC 9 Z9 9 U1 1 U2 2 PU SPRINGER/PLENUM PUBLISHERS PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0022-2291 J9 J LOW TEMP PHYS JI J. Low Temp. Phys. PD APR PY 2008 VL 151 IS 1-2 BP 138 EP 143 DI 10.1007/s10909-007-9623-3 PG 6 WC Physics, Applied; Physics, Condensed Matter SC Physics GA 270CP UT WOS:000253697900020 ER PT J AU Barrentine, EM Timbie, PT Stevenson, TR Ali, S Chervenak, JA Wollack, E Moseley, SH Allen, CA Hseih, WT Miller, TM Benford, DJ Brown, AD AF Barrentine, E. M. Timbie, P. T. Stevenson, T. R. Ali, S. Chervenak, J. A. Wollack, E. Moseley, S. H. Allen, C. A. Hseih, W. T. Miller, T. M. Benford, D. J. Brown, A. D. TI Sensitivity measurements of a transition-edge hot-electron microbolometer for millimeter-wave astrophysical observations SO JOURNAL OF LOW TEMPERATURE PHYSICS LA English DT Article; Proceedings Paper CT 12th International Workshop on Low Temperature Detectors CY JUL 22-27, 2007 CL Paris, FRANCE DE microbolometers; transition-edge sensors; cosmic microwave background; millimeter waves; hot-electron effect; transition-edge hot-electron microbolometer AB Future experiments to probe the Cosmic Microwave Background (CMB) polarization will need arrays of 1000s of sensitive bolometers. We are developing a Transition-edge Hot-electron Microbolometer (THM) to fill this need. This small-volume bolometer consists of a superconducting bilayer Transition-Edge Sensor (TES) with a thin-film absorber. Unlike traditional monolithic bolometers which make use of micromachined structures, the THM employs the decoupling between electrons and phonons at milliKelvin temperatures to provide thermal isolation. The devices are fabricated photolithographically and are easily integrated with antennas via microstrip transmission lines, and with SQUID readouts. We present the results of noise, responsivity, and thermal conductance measurements in which electrical power is dissipated in the absorber, and confirm a thermal model for a test THM with a Mo/Au TES and Bi/Au absorber. C1 [Barrentine, E. M.; Timbie, P. T.] Univ Wisconsin, Madison, WI 53706 USA. [Stevenson, T. R.; Chervenak, J. A.; Wollack, E.; Moseley, S. H.; Allen, C. A.; Hseih, W. T.; Miller, T. M.; Benford, D. J.; Brown, A. D.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Ali, S.] Lawrence Livermore Natl Lab, Livermore, CA 94550 USA. RP Barrentine, EM (reprint author), Univ Wisconsin, Madison, WI 53706 USA. EM barrentine@wisc.edu RI Brown, Ari/B-1693-2008; Benford, Dominic/D-4760-2012; Moseley, Harvey/D-5069-2012; Wollack, Edward/D-4467-2012 OI Benford, Dominic/0000-0002-9884-4206; Wollack, Edward/0000-0002-7567-4451 NR 13 TC 7 Z9 7 U1 0 U2 3 PU SPRINGER/PLENUM PUBLISHERS PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0022-2291 J9 J LOW TEMP PHYS JI J. Low Temp. Phys. PD APR PY 2008 VL 151 IS 1-2 BP 173 EP 179 DI 10.1007/s10909-007-9615-3 PG 7 WC Physics, Applied; Physics, Condensed Matter SC Physics GA 270CP UT WOS:000253697900026 ER PT J AU Smith, SJ Bandler, SR Brown, AD Chervenak, JA Figueroa-Feliciano, E Finkbeiner, F Iyomoto, N Kelley, RL Kilbourne, CA Porter, FS Sadleir, JE AF Smith, S. J. Bandler, S. R. Brown, A. -D. Chervenak, J. A. Figueroa-Feliciano, E. Finkbeiner, F. Iyomoto, N. Kelley, R. L. Kilbourne, C. A. Porter, F. S. Sadleir, J. E. TI Characterizing the superconducting-to-normal transition in Mo/Au transition-edge sensor bilayers SO JOURNAL OF LOW TEMPERATURE PHYSICS LA English DT Article; Proceedings Paper CT 12th International Workshop on Low Temperature Detectors CY JUL 22-27, 2007 CL Paris, FRANCE DE excess noise; critical current; Ginzburg-Landau ID NOISE AB We are developing arrays of Mo/Au bilayer transition-edge sensors (TES's) for future X-ray astronomy missions such as NASA's Constellation-X. The physical properties of the superconducting-to-normal transition in our TES bilayers, while often reproducible and characterized, are not well understood. The addition of normal metal features on top of the bilayer are found to change the shape and temperature of the transition, and they typically reduce the unexplained 'excess' noise. In order to understand and potentially optimize the properties of the transition, we have been studying the temperature, widths and current dependence of these transitions. We report on the characterization of devices both deposited on silicon substrates and suspended on thin silicon nitride membranes. This includes key device parameters such as the logarithmic resistance sensitivity with temperature alpha, and the logarithmic resistance sensitivity with current beta, and their correlation with excess noise. C1 [Smith, S. J.; Bandler, S. R.; Brown, A. -D.; Chervenak, J. A.; Finkbeiner, F.; Iyomoto, N.; Kelley, R. L.; Kilbourne, C. A.; Porter, F. S.; Sadleir, J. E.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Figueroa-Feliciano, E.] MIT, Kavli Inst Space Res, Cambridge, MA 02139 USA. RP Smith, SJ (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. EM sjs@milkyway.gsfc.nasa.gov RI Brown, Ari/B-1693-2008; Bandler, Simon/A-6258-2010; Smith, Stephen/B-1256-2008; Porter, Frederick/D-3501-2012; Kelley, Richard/K-4474-2012 OI Bandler, Simon/0000-0002-5112-8106; Smith, Stephen/0000-0003-4096-4675; Porter, Frederick/0000-0002-6374-1119; NR 6 TC 12 Z9 12 U1 0 U2 8 PU SPRINGER/PLENUM PUBLISHERS PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0022-2291 J9 J LOW TEMP PHYS JI J. Low Temp. Phys. PD APR PY 2008 VL 151 IS 1-2 BP 195 EP 200 DI 10.1007/s10909-007-9619-z PG 6 WC Physics, Applied; Physics, Condensed Matter SC Physics GA 270CP UT WOS:000253697900030 ER PT J AU Kilbourne, CA Bandler, SR Brown, AD Chervenak, A Figueroa-Feliciano, E Finkbeiner, F Iyomoto, N Kelley, RL Porter, FS Smith, SJ AF Kilbourne, C. A. Bandler, S. R. Brown, A. -D. Chervenak, A. Figueroa-Feliciano, E. Finkbeiner, F. Iyomoto, N. Kelley, R. L. Porter, F. S. Smith, S. J. TI Various optimizations of TES arrays for X-ray astrophysics SO JOURNAL OF LOW TEMPERATURE PHYSICS LA English DT Article; Proceedings Paper CT 12th International Workshop on Low Temperature Detectors CY JUL 22-27, 2007 CL Paris, FRANCE DE X-ray spectroscopy; X-ray calorimeter; transition-edge sensor ID RESOLUTION; LINES; SPECTROMETER; SPECTROSCOPY AB We are developing arrays of superconducting transition-edge sensors (TES) for imaging X-ray spectroscopy telescopes such as the XMS on Constellation-X. While our primary focus has been on arrays that meet the XMS requirements (of which, foremost, are an energy resolution of 2.5 eV at 6 keV and a band pass from similar to 0.3 keV to 12 keV), we are also beginning to investigate other optimizations that might be used to extend the XMS capabilities. In one of these optimizations, improved resolution below 1 keV is achieved by reducing the heat capacity. These low-energy pixels can be added to an array with broadband response either as a separate array or interspersed, depending on other factors that include telescope design and science requirements. To explore optimizations for higher count rates, we are also optimizing the design and operating temperature of pixels that are coupled to a solid substrate. We present analysis of the preliminary performance of such variations. C1 [Kilbourne, C. A.; Bandler, S. R.; Brown, A. -D.; Chervenak, A.; Finkbeiner, F.; Iyomoto, N.; Kelley, R. L.; Porter, F. S.; Smith, S. J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Bandler, S. R.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Figueroa-Feliciano, E.] MIT, Dept Phys, Cambridge, MA 02139 USA. [Finkbeiner, F.] RS Informat Syst Inc, Mclean, VA 22102 USA. [Iyomoto, N.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. RP Kilbourne, CA (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. EM Caroline.A.Kilbourne@nasa.gov RI Brown, Ari/B-1693-2008; Bandler, Simon/A-6258-2010; Smith, Stephen/B-1256-2008; Porter, Frederick/D-3501-2012; Kelley, Richard/K-4474-2012 OI Bandler, Simon/0000-0002-5112-8106; Smith, Stephen/0000-0003-4096-4675; Porter, Frederick/0000-0002-6374-1119; NR 12 TC 10 Z9 10 U1 0 U2 6 PU SPRINGER/PLENUM PUBLISHERS PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0022-2291 J9 J LOW TEMP PHYS JI J. Low Temp. Phys. PD APR PY 2008 VL 151 IS 1-2 BP 223 EP 228 DI 10.1007/s10909-007-9643-z PG 6 WC Physics, Applied; Physics, Condensed Matter SC Physics GA 270CP UT WOS:000253697900035 ER PT J AU Chervenak, JA Finkbeiner, FM Bandler, SR Brekosky, R Brown, AD Iyomoto, N Kelley, RL Kilbourne, CA Porter, FS Sadleir, J Smith, S AF Chervenak, J. A. Finkbeiner, F. M. Bandler, S. R. Brekosky, R. Brown, A. D. Iyomoto, N. Kelley, R. L. Kilbourne, C. A. Porter, F. S. Sadleir, J. Smith, S. TI Materials development for auxiliary components for large compact Mo/Au TES arrays SO JOURNAL OF LOW TEMPERATURE PHYSICS LA English DT Article; Proceedings Paper CT 12th International Workshop on Low Temperature Detectors CY JUL 22-27, 2007 CL Paris, FRANCE DE X-ray microcalorimeter; superconducting detector; heatsinking; crosstalk AB Pursuing the feasibility of scaling conventionally-micromachined transition-edge-sensor (TES) arrays, we have undertaken a study of materials suitable for array integration. A potential limitation of increased pixel count is adequate heatsinking of each detector element to its base temperature. We describe technical approaches for heat sinking large compact TES microcalorimeter arrays and calculate the achievable heatsinking based on measured material parameters. Techniques include backside-deposited thick film copper on arrays with deep-etched wells in the substrates and electroplated gold and copper-filled micro-trenches on the substrate surface. Another limitation is the sensitivity of the thin film circuit elements to applied stress, which can arise in fabrication and mounting of arrays of increasing size. We have explored stress and deposition temperature sensitivity in our molybdenum-based bilayers. Such process parameters can impact options for array heat sinking and electrical interconnects. C1 [Chervenak, J. A.; Finkbeiner, F. M.; Bandler, S. R.; Brekosky, R.; Brown, A. D.; Iyomoto, N.; Kelley, R. L.; Kilbourne, C. A.; Porter, F. S.; Sadleir, J.; Smith, S.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Chervenak, JA (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. EM James.A.Chervenak@nasa.gov RI Brown, Ari/B-1693-2008; Bandler, Simon/A-6258-2010; Smith, Stephen/B-1256-2008; Porter, Frederick/D-3501-2012; Kelley, Richard/K-4474-2012 OI Bandler, Simon/0000-0002-5112-8106; Smith, Stephen/0000-0003-4096-4675; Porter, Frederick/0000-0002-6374-1119; NR 6 TC 6 Z9 6 U1 0 U2 4 PU SPRINGER/PLENUM PUBLISHERS PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0022-2291 J9 J LOW TEMP PHYS JI J. Low Temp. Phys. PD APR PY 2008 VL 151 IS 1-2 BP 255 EP 260 DI 10.1007/s10909-007-9636-y PG 6 WC Physics, Applied; Physics, Condensed Matter SC Physics GA 270CP UT WOS:000253697900041 ER PT J AU Allen, CA Benford, DJ Miller, TM Moseley, SH Staguhn, JG Wollack, EJ AF Allen, C. A. Benford, D. J. Miller, T. M. Moseley, S. H. Staguhn, J. G. Wollack, E. J. TI Design and fabrication highlights enabling a 2 mm, 128 element bolometer array for GISMO SO JOURNAL OF LOW TEMPERATURE PHYSICS LA English DT Article; Proceedings Paper CT 12th International Workshop on Low Temperature Detectors CY JUL 22-27, 2007 CL Paris, FRANCE DE bolometer array; transition edge sensor ID TES BOLOMETERS AB The Backshort-Under-Grid (BUG) superconducting bolometer array architecture is intended to be highly versatile, operating over a large range of wavelengths and background conditions. To validate the basic array design and to demonstrate its applicability for future kilopixel arrays, we will demonstrate a 128-element bolometer array optimized for 2 mm wavelength using a new Goddard Space Flight Center instrument, GISMO (Goddard IRAM Superconducting 2-Millimeter Observer). The design considerations unique to GISMO and laboratory experimental results will be discussed. C1 [Allen, C. A.; Benford, D. J.; Miller, T. M.; Moseley, S. H.; Staguhn, J. G.; Wollack, E. J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Allen, CA (reprint author), NASA, Goddard Space Flight Ctr, Code 553, Greenbelt, MD 20771 USA. EM christine.a.allen@nasa.gov RI Benford, Dominic/D-4760-2012; Moseley, Harvey/D-5069-2012; Wollack, Edward/D-4467-2012 OI Benford, Dominic/0000-0002-9884-4206; Wollack, Edward/0000-0002-7567-4451 NR 8 TC 1 Z9 1 U1 1 U2 1 PU SPRINGER/PLENUM PUBLISHERS PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0022-2291 J9 J LOW TEMP PHYS JI J. Low Temp. Phys. PD APR PY 2008 VL 151 IS 1-2 BP 266 EP 270 DI 10.1007/s10909-007-9646-9 PG 5 WC Physics, Applied; Physics, Condensed Matter SC Physics GA 270CP UT WOS:000253697900043 ER PT J AU Burck, A Kempf, S Schafer, S Rotzinger, H Rodrigues, M Wolf, T Gastaldo, L Fleischmann, A Enss, C AF Burck, A. Kempf, S. Schafer, S. Rotzinger, H. Rodrigues, M. Wolf, T. Gastaldo, L. Fleischmann, A. Enss, C. TI Microstructured magnetic calorimeter with meander-shaped pickup coil SO JOURNAL OF LOW TEMPERATURE PHYSICS LA English DT Article; Proceedings Paper CT 12th International Workshop on Low Temperature Detectors CY JUL 22-27, 2007 CL Paris, FRANCE DE MMC; metallic magnetic calorimeter; low temperature detectors; rare earth alloys; gold-erbium alloy; x-ray spectroscopy AB In the last years metallic magnetic calorimeters (MMC) showed an energy resolution of a few eV for x-rays up to 10 keV. This makes MMCs a promising and powerful tool for many applications where photons or energetic massive particles have to be detected-like absolute activity measurements of radioactive isotopes, high resolution x-ray spectroscopy and x-ray fluorescence material analysis. However, in order to fulfill all requirements of these applications and to allow to reach the maximum resolving power a consequent micro-fabrication of the MMC detectors is needed. The micro-fabrication of metallic magnetic calorimeters requires reliable deposition and patterning processes for niobium structures with high critical currents and for paramagnetic sensors. As one result of our advances in microstructuring a fully microfabricated MMC which consists of a meander shaped niobium thin film pickup coil and a 3 mu m thick sputter deposited paramagnetic Au:Er temperature sensor will be presented. Deposition of energy in the paramagnetic sensor causes a rise in temperature and results in a change of magnetization, which is measured by a low noise high bandwidth dc-SQUID. The sputter deposited Au:Er films we report on are working well and show thermodynamic properties close to the ones known from bulk material down to temperatures of 45 mK. C1 [Burck, A.; Kempf, S.; Schafer, S.; Wolf, T.; Gastaldo, L.; Fleischmann, A.; Enss, C.] Univ Heidelberg, Kirchhoff Inst Phys, D-69120 Heidelberg, Germany. [Rotzinger, H.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Rotzinger, H.] Brown Univ, Greenbelt, MD 20771 USA. [Rodrigues, M.] CEA Saclay, DETECS, DRT, Lab Natl Henri Becquerel, F-91191 Gif Sur Yvette, France. RP Burck, A (reprint author), Univ Heidelberg, Kirchhoff Inst Phys, INF 227, D-69120 Heidelberg, Germany. EM Andreas.Burck@kip.uni-heidelberg.de RI Kempf, Sebastian/P-7612-2016 OI Kempf, Sebastian/0000-0002-3303-128X NR 6 TC 19 Z9 19 U1 0 U2 1 PU SPRINGER/PLENUM PUBLISHERS PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0022-2291 J9 J LOW TEMP PHYS JI J. Low Temp. Phys. PD APR PY 2008 VL 151 IS 1-2 BP 337 EP 344 DI 10.1007/s10909-007-9659-4 PG 8 WC Physics, Applied; Physics, Condensed Matter SC Physics GA 270CP UT WOS:000253697900055 ER PT J AU Rotzinger, H Adams, J Bandler, SR Beyer, J Eguchi, H Figueroa-Feliciano, E Hsieh, W Seidel, GM Stevenson, T AF Rotzinger, H. Adams, J. Bandler, S. R. Beyer, J. Eguchi, H. Figueroa-Feliciano, E. Hsieh, W. Seidel, G. M. Stevenson, T. TI Performance of micro-fabricated magnetic calorimeters arrays for X-ray spectroscopy SO JOURNAL OF LOW TEMPERATURE PHYSICS LA English DT Article; Proceedings Paper CT 12th International Workshop on Low Temperature Detectors CY JUL 22-27, 2007 CL Paris, FRANCE DE magnetic calorimeter; X-ray spectroscopy; low temperature detector AB We have been developing array technology for fabricating magnetic calorimeters for X-ray astronomy. The magnetization change in each pixel of the paramagnetic sensor material due to the heat input of an absorbed X-ray is sensed by a meander shaped coil. With this geometry it is possible to obtain excellent energy sensitivity, low magnetic cross-talk and large format arrays fabricated on wafers that are separate from the SQUID read-out. A magnetic bias field for each pixel is generated by the use of a persistent current that is stored. We report on the results from our prototype arrays, which are coupled to low noise DC-SQUIDs. The first test results are presented and the sensitivity is compared with calculations. C1 [Rotzinger, H.; Adams, J.; Bandler, S. R.; Hsieh, W.; Stevenson, T.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Beyer, J.] Phys Tech Bundesanstalt, Berlin, Germany. [Figueroa-Feliciano, E.] MIT, Boston, MA USA. [Rotzinger, H.; Eguchi, H.; Seidel, G. M.] Brown Univ, Providence, RI 02912 USA. RP Rotzinger, H (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. EM hannes.rotzinger@milkyway.gsfc.nasa.gov RI Bandler, Simon/A-6258-2010 OI Bandler, Simon/0000-0002-5112-8106 NR 3 TC 12 Z9 12 U1 0 U2 2 PU SPRINGER/PLENUM PUBLISHERS PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0022-2291 J9 J LOW TEMP PHYS JI J. Low Temp. Phys. PD APR PY 2008 VL 151 IS 1-2 BP 351 EP 356 DI 10.1007/s10909-007-9658-5 PG 6 WC Physics, Applied; Physics, Condensed Matter SC Physics GA 270CP UT WOS:000253697900057 ER PT J AU Hsieh, WT Adams, JA Bandler, SR Beyer, J Denis, KL Eguchi, H Figueroa-Feliciano, E Rotzinger, H Schneider, GH Seidel, GM Stevenson, TR Travers, DE AF Hsieh, W. -T. Adams, J. A. Bandler, S. R. Beyer, J. Denis, K. L. Eguchi, H. Figueroa-Feliciano, E. Rotzinger, H. Schneider, G. H. Seidel, G. M. Stevenson, T. R. Travers, D. E. TI Fabrication of metallic magnetic calorimeter X-ray detector arrays SO JOURNAL OF LOW TEMPERATURE PHYSICS LA English DT Article; Proceedings Paper CT 12th International Workshop on Low Temperature Detectors CY JUL 22-27, 2007 CL Paris, FRANCE DE magnetic calorimeter; X-ray detector; AuEr film AB Microcalorimeters with metallic magnetic sensors show great promise for use in astronomical X-ray spectroscopy. We describe the design and fabrication of a lithographically patterned magnetic microcalorimeter. A paramagnetic AuEr film is sputter-deposited as the sensor, which is coupled to a low noise SQUID via a meander superconducting pickup loop used as an inductor. This inductor also provides the magnetic field bias to the sensor. The AuEr film is deposited over this meander such that the field created by a large current flowing in the loop magnetizes the sensor material. The use of thin film techniques in the fabrication of these magnetic sensors not only allows strong magnetic coupling between the sensor and the inductor, it also is scalable for array fabrication. C1 [Hsieh, W. -T.; Adams, J. A.; Bandler, S. R.; Denis, K. L.; Rotzinger, H.; Schneider, G. H.; Stevenson, T. R.; Travers, D. E.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Beyer, J.] Phys Tech Bundesanstalt, Inst Berlin, D-10587 Berlin, Germany. [Eguchi, H.; Seidel, G. M.] Brown Univ, Dept Phys, Providence, RI 02912 USA. [Figueroa-Feliciano, E.] MIT, Dept Phys, Cambridge, MA 02139 USA. RP Hsieh, WT (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. EM wen-ting.hsieh-1@nasa.gov RI Bandler, Simon/A-6258-2010 OI Bandler, Simon/0000-0002-5112-8106 NR 4 TC 10 Z9 10 U1 2 U2 2 PU SPRINGER/PLENUM PUBLISHERS PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0022-2291 J9 J LOW TEMP PHYS JI J. Low Temp. Phys. PD APR PY 2008 VL 151 IS 1-2 BP 357 EP 362 DI 10.1007/s10909-007-9661-x PG 6 WC Physics, Applied; Physics, Condensed Matter SC Physics GA 270CP UT WOS:000253697900058 ER PT J AU Kelley, RL Allen, CA Galeazzi, M Kilbourne, CA McCammon, D Porter, FS Szymkowiak, AE AF Kelley, R. L. Allen, C. A. Galeazzi, M. Kilbourne, C. A. McCammon, D. Porter, F. S. Szymkowiak, A. E. TI Ion-implanted silicon X-ray calorimeters: Present and future SO JOURNAL OF LOW TEMPERATURE PHYSICS LA English DT Article; Proceedings Paper CT 12th International Workshop on Low Temperature Detectors CY JUL 22-27, 2007 CL Paris, FRANCE ID THERMAL DETECTORS; MICROCALORIMETER; SUZAKU AB We now have about 25 years of experience with X-ray calorimeters based on doped semiconductor thermometers. Ion-implanted Si arrays have been used in astrophysics and laboratory atomic physics. The device properties and characteristics are sufficiently well understood to allow optimized designs for a wide variety of applications over the 0.1-100 keV range. With new absorber materials, approaches for absorber attachment and compact, low thermal conductance JFET arrays, it should be possible to advance this technology from the 36 pixel arrays of today to arrays that are about an order of magnitude larger, and with significantly improved energy resolution. These would enable new capabilities on instruments being considered now for missions that may fly in about five years. C1 [Kelley, R. L.; Allen, C. A.; Kilbourne, C. A.; Porter, F. S.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Galeazzi, M.] Univ Miami, Dept Phys, Coral Gables, FL 33124 USA. [McCammon, D.] Univ Wisconsin, Dept Phys, Madison, WI 53706 USA. [Szymkowiak, A. E.] Yale Univ, Dept Phys, New Haven, CT 06511 USA. RP Kelley, RL (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. EM Richard.L.Kelley@nasa.gov RI Porter, Frederick/D-3501-2012; Kelley, Richard/K-4474-2012; XRAY, SUZAKU/A-1808-2009 OI Porter, Frederick/0000-0002-6374-1119; NR 18 TC 7 Z9 7 U1 0 U2 2 PU SPRINGER/PLENUM PUBLISHERS PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0022-2291 J9 J LOW TEMP PHYS JI J. Low Temp. Phys. PD APR PY 2008 VL 151 IS 1-2 BP 375 EP 380 DI 10.1007/s10909-007-9663-8 PG 6 WC Physics, Applied; Physics, Condensed Matter SC Physics GA 270CP UT WOS:000253697900061 ER PT J AU Bandler, SR Brekosky, RP Brown, AD Chervenak, JA Figueroa-Feliciano, E Finkbeiner, FM Iyomoto, N Kelley, RL Kilbourne, CA Porter, FS Sadleir, J Smith, SJ AF Bandler, S. R. Brekosky, R. P. Brown, A. -D. Chervenak, J. A. Figueroa-Feliciano, E. Finkbeiner, F. M. Iyomoto, N. Kelley, R. L. Kilbourne, C. A. Porter, F. S. Sadleir, J. Smith, S. J. TI Performance of TES X-ray microcalorimeters with a novel absorber design SO JOURNAL OF LOW TEMPERATURE PHYSICS LA English DT Article; Proceedings Paper CT 12th International Workshop on Low Temperature Detectors CY JUL 22-27, 2007 CL Paris, FRANCE DE microcalorimeters; transition edge sensors AB Superconducting transition-edge sensor (TES) microcalorimeters have demonstrated the Constellation-X requirements for spectral resolution, speed, and pixel size in a close-packed geometry. We will present our recent breakthrough energy resolution with sensors that have all gold and bismuth-gold absorbers. This has been enabled by cantilevered absorbers that make contact to the TES only in regions that are not part of the active thermometer. With this approach, rapid thermalization of the x-ray energy is achieved and interaction between the absorber and TES sensor films is avoided. This design allows us to obtain uniform high performance and is compatible with large-format, high fill-factor arrays. We will discuss this design, the results we have achieved in 8x8 arrays of these pixels, and the dependence of the performance on the geometry of the absorber contact area and on stress within the sensor. C1 [Bandler, S. R.; Brekosky, R. P.; Brown, A. -D.; Chervenak, J. A.; Finkbeiner, F. M.; Iyomoto, N.; Kelley, R. L.; Kilbourne, C. A.; Porter, F. S.; Sadleir, J.; Smith, S. J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Figueroa-Feliciano, E.] MIT, Kavli Inst, Cambridge, MA 02139 USA. RP Bandler, SR (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. EM Simon.R.Bandler@nasa.gov RI Brown, Ari/B-1693-2008; Bandler, Simon/A-6258-2010; Smith, Stephen/B-1256-2008; Porter, Frederick/D-3501-2012; Kelley, Richard/K-4474-2012 OI Bandler, Simon/0000-0002-5112-8106; Smith, Stephen/0000-0003-4096-4675; Porter, Frederick/0000-0002-6374-1119; NR 6 TC 56 Z9 56 U1 1 U2 12 PU SPRINGER/PLENUM PUBLISHERS PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0022-2291 J9 J LOW TEMP PHYS JI J. Low Temp. Phys. PD APR PY 2008 VL 151 IS 1-2 BP 400 EP 405 DI 10.1007/s10909-007-9673-6 PG 6 WC Physics, Applied; Physics, Condensed Matter SC Physics GA 270CP UT WOS:000253697900065 ER PT J AU Iyomoto, N Bandler, SR Brekosky, RP Brown, AD Chervenak, JA Figueroa-Feliciano, E Finkbeiner, FM Kelley, RL Kilbourne, CA Lindeman, MA Porter, FS Saab, T Sadleir, JE Smith, SJ AF Iyomoto, N. Bandler, S. R. Brekosky, R. P. Brown, A. -D. Chervenak, J. A. Figueroa-Feliciano, E. Finkbeiner, F. M. Kelley, R. L. Kilbourne, C. A. Lindeman, M. A. Porter, F. S. Saab, T. Sadleir, J. E. Smith, S. J. TI Modeling of TES X-ray microcalorimeters with a novel absorber design SO JOURNAL OF LOW TEMPERATURE PHYSICS LA English DT Article; Proceedings Paper CT 12th International Workshop on Low Temperature Detectors CY JUL 22-27, 2007 CL Paris, FRANCE DE microcalorimeters; transition edge sensors; X-ray spectroscopy ID IMPEDANCE MEASUREMENTS; CALORIMETER AB We have successfully modeled our new TES (transition-edge sensor) X-ray microcalorimeters with a novel X-ray absorber design that is suitable for close-packed array with high quantum efficiency. We have determined device parameters that reproduce complex impedance curves and noise spectra throughout the transition. Observed pulse height, decay time and baseline energy resolution were in good agreement with simulated results using the same parameters. C1 [Iyomoto, N.; Bandler, S. R.; Brekosky, R. P.; Brown, A. -D.; Chervenak, J. A.; Figueroa-Feliciano, E.; Finkbeiner, F. M.; Kelley, R. L.; Kilbourne, C. A.; Lindeman, M. A.; Porter, F. S.; Saab, T.; Sadleir, J. E.; Smith, S. J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Iyomoto, N (reprint author), NASA, Goddard Space Flight Ctr, Code 662, Greenbelt, MD 20771 USA. EM Naoko.Iyomoto@nasa.gov RI Brown, Ari/B-1693-2008; Bandler, Simon/A-6258-2010; Smith, Stephen/B-1256-2008; Porter, Frederick/D-3501-2012; Kelley, Richard/K-4474-2012 OI Bandler, Simon/0000-0002-5112-8106; Smith, Stephen/0000-0003-4096-4675; Porter, Frederick/0000-0002-6374-1119; NR 7 TC 18 Z9 18 U1 0 U2 6 PU SPRINGER/PLENUM PUBLISHERS PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0022-2291 J9 J LOW TEMP PHYS JI J. Low Temp. Phys. PD APR PY 2008 VL 151 IS 1-2 BP 406 EP 412 DI 10.1007/s10909-007-9668-3 PG 7 WC Physics, Applied; Physics, Condensed Matter SC Physics GA 270CP UT WOS:000253697900066 ER PT J AU Brown, AD Bandler, SR Brekosky, R Chervenak, JA Figueroa-Feliciano, E Finkbeiner, F Iyomoto, N Kelley, RL Kilbourne, CA Porter, FS Smith, S Saab, T Sadleir, J AF Brown, A. -D. Bandler, S. R. Brekosky, R. Chervenak, J. A. Figueroa-Feliciano, E. Finkbeiner, F. Iyomoto, N. Kelley, R. L. Kilbourne, C. A. Porter, F. S. Smith, S. Saab, T. Sadleir, J. TI Absorber materials for transition-edge sensor X-ray microcalorimeters SO JOURNAL OF LOW TEMPERATURE PHYSICS LA English DT Article; Proceedings Paper CT 12th International Workshop on Low Temperature Detectors CY JUL 22-27, 2007 CL Paris, FRANCE DE transition-edge sensors; calorimeters; electroplating ID BISMUTH AB Arrays of superconducting transition-edge sensors (TES) can provide high spatial and energy resolution necessary for X-ray astronomy. High quantum efficiency and uniformity of response can be achieved with a suitable absorber material, in which absorber X-ray stopping power, heat capacity, and thermal conductivity are relevant parameters. Here we compare these parameters for bismuth and gold. We have fabricated electroplated gold, electroplated gold/electroplated bismuth, and evaporated gold/evaporated bismuth 8 x 8 absorber arrays and find that a correlation exists between the residual resistance ratio (RRR) and thin film microstructure. This finding indicates that we can tailor absorber material conductivity via microstructure alteration, so as to permit absorber thermalization on timescales suitable for high energy resolution X-ray microcalorimetry. We show that by incorporating absorbers possessing large grain size, including electroplated gold and electroplated gold/electroplated bismuth, into our current Mo/Au TES, devices with tunable heat capacity and energy resolution of 2.4 eV (gold) and 2.1 eV (gold/bismuth) FWHM at 5.9 keV have been fabricated. C1 [Brown, A. -D.; Bandler, S. R.; Brekosky, R.; Chervenak, J. A.; Finkbeiner, F.; Iyomoto, N.; Kelley, R. L.; Kilbourne, C. A.; Porter, F. S.; Smith, S.; Sadleir, J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Figueroa-Feliciano, E.] MIT, Dept Phys, Cambridge, MA 02139 USA. [Iyomoto, N.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Saab, T.] Univ Florida, Dept Phys, Gainesville, FL 32611 USA. [Sadleir, J.] Univ Illinois, Dept Phys, Urbana, IL 61801 USA. RP Brown, AD (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. EM abrown@pop500.gsfc.nasa.gov RI Brown, Ari/B-1693-2008; Bandler, Simon/A-6258-2010; Smith, Stephen/B-1256-2008; Porter, Frederick/D-3501-2012; Kelley, Richard/K-4474-2012 OI Bandler, Simon/0000-0002-5112-8106; Smith, Stephen/0000-0003-4096-4675; Porter, Frederick/0000-0002-6374-1119; NR 7 TC 11 Z9 11 U1 2 U2 11 PU SPRINGER/PLENUM PUBLISHERS PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0022-2291 J9 J LOW TEMP PHYS JI J. Low Temp. Phys. PD APR PY 2008 VL 151 IS 1-2 BP 413 EP 417 DI 10.1007/s10909-007-9669-2 PG 5 WC Physics, Applied; Physics, Condensed Matter SC Physics GA 270CP UT WOS:000253697900067 ER PT J AU Moseley, SJ Allen, CA Costin, N Kelley, R Kilbourne, C Miller, T AF Moseley, Samuel J. Allen, Christine A. Costin, Nicholas Kelley, Richard Kilbourne, Caroline Miller, Timothy TI Automated hybridization of X-ray absorber elements a path to large format microcalorimeter arrays SO JOURNAL OF LOW TEMPERATURE PHYSICS LA English DT Article; Proceedings Paper CT 12th International Workshop on Low Temperature Detectors CY JUL 22-27, 2007 CL Paris, FRANCE DE X-ray absorbers; mercury telluride; SU-8; automated tile application; adhesive attachment; XeF2 etching AB We have developed an automated die-scale process for the attachment of X-ray absorbers onto microcalorimeters. Here, we describe the process for the production of absorber tiles on a handle wafer, their attachment to the microcalorimeter, and the removal of the supporting handle wafer. The process is shown to be a robust path to large format arrays of microcalorimeters. C1 [Moseley, Samuel J.; Allen, Christine A.; Costin, Nicholas; Kelley, Richard; Kilbourne, Caroline; Miller, Timothy] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20772 USA. [Moseley, Samuel J.; Costin, Nicholas; Miller, Timothy] MEI Technol Inc, Seabrook, MD 20706 USA. RP Moseley, SJ (reprint author), NASA, Goddard Space Flight Ctr, Code 553,8800 Greenbelt Rd, Greenbelt, MD 20772 USA. EM sjmosele@pop500.gsfc.nasa.gov RI Kelley, Richard/K-4474-2012 NR 2 TC 1 Z9 1 U1 0 U2 0 PU SPRINGER/PLENUM PUBLISHERS PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0022-2291 J9 J LOW TEMP PHYS JI J. Low Temp. Phys. PD APR PY 2008 VL 151 IS 1-2 BP 418 EP 423 DI 10.1007/s10909-007-9670-9 PG 6 WC Physics, Applied; Physics, Condensed Matter SC Physics GA 270CP UT WOS:000253697900068 ER PT J AU Figueroa-Feliciano, E Saab, T Rivera-Ortiz, PM Bandler, SR Iyomoto, N Kelley, RL Kilbourne, CA Porter, FS Smith, SJ AF Figueroa-Feliciano, E. Saab, T. Rivera-Ortiz, P. M. Bandler, S. R. Iyomoto, N. Kelley, R. L. Kilbourne, C. A. Porter, F. S. Smith, S. J. TI Studies of thermal diffusion in planar absorber designs for the Micro-X rocket SO JOURNAL OF LOW TEMPERATURE PHYSICS LA English DT Article; Proceedings Paper CT 12th International Workshop on Low Temperature Detectors CY JUL 22-27, 2007 CL Paris, FRANCE DE TES; microcalorimeter; Micro-X; diffusion; position dependence AB We have studied a potential design for a transition-edge sensor (TES) microcalorimeter array for the Micro-X High Resolution Microcalorimeter X-ray Imaging Rocket. Diffusion simulations of a design that places a small TES in the center of the pixel with a large in-plane absorber around the TES demonstrate that with high-quality gold films (RRR > 6) 2 eV resolution is attainable in a 700 mu m pixel, meeting the Micro-X requirement. X-ray hits directly on the TES, however, create a non-gaussian high energy tail to the device response. This high energy tail contains 5% of incident photons and cannot be removed by lowering the optimal filter bandwidth. C1 [Figueroa-Feliciano, E.] MIT, Dept Phys, Cambridge, MA 02139 USA. [Saab, T.] Univ Florida, Dept Phys, Gainesville, FL 32611 USA. [Rivera-Ortiz, P. M.] Univ Puerto Rico, Dept Mech Engn, Mayaguez, PR 00680 USA. [Bandler, S. R.; Iyomoto, N.; Kelley, R. L.; Kilbourne, C. A.; Porter, F. S.; Smith, S. J.] NASA, Goddard Space Flight Ctr, Xray Astrophys Lab, Greenbelt, MD 20771 USA. RP Figueroa-Feliciano, E (reprint author), MIT, Dept Phys, Cambridge, MA 02139 USA. EM enectali@mit.edu RI Bandler, Simon/A-6258-2010; Smith, Stephen/B-1256-2008; Porter, Frederick/D-3501-2012; Kelley, Richard/K-4474-2012 OI Bandler, Simon/0000-0002-5112-8106; Smith, Stephen/0000-0003-4096-4675; Porter, Frederick/0000-0002-6374-1119; NR 2 TC 2 Z9 2 U1 0 U2 2 PU SPRINGER/PLENUM PUBLISHERS PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0022-2291 J9 J LOW TEMP PHYS JI J. Low Temp. Phys. PD APR PY 2008 VL 151 IS 1-2 BP 424 EP 429 DI 10.1007/s10909-007-9667-4 PG 6 WC Physics, Applied; Physics, Condensed Matter SC Physics GA 270CP UT WOS:000253697900069 ER PT J AU Stevenson, T Benford, D Bennett, C Cao, N Chuss, D Denis, K Hsieh, W Kogut, A Moseley, S Panek, J Schneider, G Travers, D U-Yen, K Voellmer, G Wollack, E AF Stevenson, T. Benford, D. Bennett, C. Cao, N. Chuss, D. Denis, K. Hsieh, W. Kogut, A. Moseley, S. Panek, J. Schneider, G. Travers, D. U-Yen, K. Voellmer, G. Wollack, E. TI Cosmic microwave background polarization detector with high efficiency, broad bandwidth, and highly symmetric coupling to transition edge sensor bolometers SO JOURNAL OF LOW TEMPERATURE PHYSICS LA English DT Article; Proceedings Paper CT 12th International Workshop on Low Temperature Detectors CY JUL 22-27, 2007 CL Paris, FRANCE DE polarimeter; microstrip; aluminum oxide; loss tangent; thin film; microwave modeling ID QUANTUM INTERFERENCE DEVICE; ARRAYS; TIME AB We describe a prototype detector system designed for precise measurements of Cosmic Microwave Background polarization. The design combines a quasi-optical polarization modulator, a metal feedhorn, a superconducting planar microwave circuit, and a pair of transition-edge sensor (TES) bolometers operating at < 100 mK. The circular feedhorn produces highly symmetric beams with very low cross-polarization. The planar circuit preserves symmetry in coupling to bolometers measuring orthogonal polarizations. We implement the circuit with superconducting niobium transmission lines. Three-dimensional interfaces between the planar circuit and waveguides leading to feedhorn and backshort have been carefully designed with electromagnetic simulations. Power is thermalized in resistors and conducted to bolometers via normal electrons. Our system is designed for a 29-43 GHz signal band. We have tested individual circuit elements in this frequency range. Fabrication of a full single-pixel system is underway. C1 [Stevenson, T.; Benford, D.; Cao, N.; Chuss, D.; Denis, K.; Hsieh, W.; Kogut, A.; Moseley, S.; Panek, J.; Schneider, G.; Travers, D.; U-Yen, K.; Voellmer, G.; Wollack, E.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Bennett, C.] Johns Hopkins Univ, Dept Phys, Baltimore, MD 21218 USA. RP Stevenson, T (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. EM thomas.r.stevenson@nasa.gov RI Benford, Dominic/D-4760-2012; Moseley, Harvey/D-5069-2012; Kogut, Alan/D-6293-2012; Wollack, Edward/D-4467-2012 OI Benford, Dominic/0000-0002-9884-4206; Wollack, Edward/0000-0002-7567-4451 NR 22 TC 7 Z9 7 U1 0 U2 2 PU SPRINGER/PLENUM PUBLISHERS PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0022-2291 EI 1573-7357 J9 J LOW TEMP PHYS JI J. Low Temp. Phys. PD APR PY 2008 VL 151 IS 1-2 BP 471 EP 476 DI 10.1007/s10909-007-9679-0 PG 6 WC Physics, Applied; Physics, Condensed Matter SC Physics GA 270CP UT WOS:000253697900076 ER PT J AU Day, P Leduc, HG Dowell, CD Lee, RA Turner, A Zmuidzinas, J AF Day, P. Leduc, H. G. Dowell, C. D. Lee, R. A. Turner, A. Zmuidzinas, J. TI Distributed antenna-coupled TES for FIR detector arrays SO JOURNAL OF LOW TEMPERATURE PHYSICS LA English DT Article; Proceedings Paper CT 12th International Workshop on Low Temperature Detectors CY JUL 22-27, 2007 CL Paris, FRANCE DE TES; antenna; FIR ID METALS AB We report progress toward large arrays of sensitive TES bolometers for submillimeter and far-infrared wavelengths with noise equivalent power (NEP) suitable for either imaging from a cooled space telescope or ground based spectroscopy. The arrays are based on a pixel design that makes use of a distributed transition edge sensor (TES) coupled to a slot antenna array. We have electrically characterized prototype detectors consisting of 256 TiN hot-electron TES microbolometers biased in parallel with T (c) =50 mK. The measured electron-phonon thermal conductance of prototype devices is as low as 1.1 pW/K at 50 mK corresponding to an electrical NEP of 4x10(-19) W/Hz(1/2). The time constant of two detectors with different geometries and transition widths was measured under a range of bias conditions. We have measured time constants greater than or similar to 10(-3) seconds, which is long enough for straightforward multiplexing with existing multiplexer technology. C1 [Day, P.; Leduc, H. G.; Dowell, C. D.; Lee, R. A.; Turner, A.; Zmuidzinas, J.] Jet Propuls Lab, Pasadena, CA 91109 USA. RP Day, P (reprint author), Jet Propuls Lab, Pasadena, CA 91109 USA. EM Peter.K.Day@jpl.nasa.gov NR 8 TC 6 Z9 6 U1 2 U2 4 PU SPRINGER/PLENUM PUBLISHERS PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0022-2291 J9 J LOW TEMP PHYS JI J. Low Temp. Phys. PD APR PY 2008 VL 151 IS 1-2 BP 477 EP 482 DI 10.1007/s10909-007-9676-3 PG 6 WC Physics, Applied; Physics, Condensed Matter SC Physics GA 270CP UT WOS:000253697900077 ER PT J AU Miller, TM Costen, N Allen, C AF Miller, Timothy M. Costen, Nick Allen, Christine TI Indium hybridization of large format TES bolometer arrays to readout multiplexers for far-infrared astronomy SO JOURNAL OF LOW TEMPERATURE PHYSICS LA English DT Article; Proceedings Paper CT 12th International Workshop on Low Temperature Detectors CY JUL 22-27, 2007 CL Paris, FRANCE DE indium; hybridization; TES; bolometer; infrared; astronomy ID FABRICATION; SCUBA-2 AB In our effort to develop large format kilo-pixel arrays of transition edge sensors, we are working toward demonstrating electrical connectivity of a hybridized 32x40 element detector to a NIST multiplexer. The geometry of large-scale arrays that attempt to maintain a high filling factor does not allow for typical fan-out wiring, thus the detector array is hybridized directly to the readout multiplexer. The two parts are bonded together with 10 micron tall indium bumps, which complete the electrical path and also provide mechanical strength. The indium hybridization was developed and performed at the Goddard Space Flight Center and has been shown to withstand tensile loading up to 0.26 gram-force per indium bump. A cavity is deep etched behind each pixel prior to bonding, leaving only 30 micron support walls, which maintains a high filling fraction. Electrical continuity has been shown through the indium path in room temperature measurements. We report on the fabrication process used to hybridize the parts and the subsequent electrical performance. C1 [Miller, Timothy M.; Costen, Nick; Allen, Christine] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Miller, TM (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. EM timothy.m.miller@nasa.gov NR 9 TC 6 Z9 6 U1 0 U2 1 PU SPRINGER/PLENUM PUBLISHERS PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0022-2291 J9 J LOW TEMP PHYS JI J. Low Temp. Phys. PD APR PY 2008 VL 151 IS 1-2 BP 483 EP 488 DI 10.1007/s10909-007-9677-2 PG 6 WC Physics, Applied; Physics, Condensed Matter SC Physics GA 270CP UT WOS:000253697900078 ER PT J AU Silverberg, RF Benford, DJ Chen, T Chervenak, J Finkbeiner, FM Miller, NA Schmidt, D Ullom, JN AF Silverberg, R. F. Benford, D. J. Chen, T. Chervenak, J. Finkbeiner, F. M. Miller, N. A. Schmidt, D. Ullom, J. N. TI Superconducting transition-edge sensor bolometers with integrated electron-tunneling refrigerators SO JOURNAL OF LOW TEMPERATURE PHYSICS LA English DT Article; Proceedings Paper CT 12th International Workshop on Low Temperature Detectors CY JUL 22-27, 2007 CL Paris, FRANCE DE tunneling; NIS refrigerator; TES bolometer ID NOISE AB We discuss the development of an array of superconducting Transition-Edge Sensor (TES) bolometers intended for use at millimeter wavelengths. Each bolometer in the array uses a proximity-effect TES sensing element and each has integrated Normal-Insulator-Superconductor (NIS) refrigerators to cool the bolometer below the reference bath temperature. The NIS refrigerators and bolometers are fabricated on a single Silicon substrate. Four short, thin and narrow legs suspend the millimeter wavelength radiation-absorbing element. The leg geometry is used to control and optimize the thermal conductance of the bolometer. Using the technology developed at NIST, we fabricated NIS refrigerators at the base of each of the suspension legs. These NIS refrigerators remove hot electrons by quantum-mechanical tunneling and should be capable of reducing the temperature of the biased (similar to 10 pW) bolometers by more than 100 mK when operating from a local thermal reservoir provided by a He-3 system at similar to 300 mK. This lower temperature at the bolometer will allow the detectors to approach background-limited performance despite the simple cryogenic system. In this paper we describe the progress toward the development of these detectors designed for use in observations at the 100 m Green Bank Telescope at 3 mm wavelength and the results of laboratory tests of a prototype detector. C1 [Silverberg, R. F.; Benford, D. J.; Chen, T.; Chervenak, J.; Finkbeiner, F. M.; Miller, N. A.; Schmidt, D.; Ullom, J. N.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Silverberg, RF (reprint author), NASA, Goddard Space Flight Ctr, Code 665, Greenbelt, MD 20771 USA. EM robert.silverberg@nasa.gov RI Tomlin, Nathan/A-4927-2009; Benford, Dominic/D-4760-2012 OI Tomlin, Nathan/0000-0002-8313-9045; Benford, Dominic/0000-0002-9884-4206 NR 6 TC 1 Z9 1 U1 0 U2 5 PU SPRINGER/PLENUM PUBLISHERS PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0022-2291 J9 J LOW TEMP PHYS JI J. Low Temp. Phys. PD APR PY 2008 VL 151 IS 1-2 BP 489 EP 494 DI 10.1007/s10909-007-9674-5 PG 6 WC Physics, Applied; Physics, Condensed Matter SC Physics GA 270CP UT WOS:000253697900079 ER PT J AU Iyomoto, N Bandler, SR Brekosky, RP Brown, AD Chervenak, JA Figueroa-Feliciano, E Finkbeiner, FM Kelley, RL Kilbourne, CA Porter, FS Sadleir, JE Smith, SJ AF Iyomoto, N. Bandler, S. R. Brekosky, R. P. Brown, A. -D. Chervenak, J. A. Figueroa-Feliciano, E. Finkbeiner, F. M. Kelley, R. L. Kilbourne, C. A. Porter, F. S. Sadleir, J. E. Smith, S. J. TI Heat sinking and crosstalk for large, close-packed arrays of microcalorimeters SO JOURNAL OF LOW TEMPERATURE PHYSICS LA English DT Article; Proceedings Paper CT 12th International Workshop on Low Temperature Detectors CY JUL 22-27, 2007 CL Paris, FRANCE DE microcalorimeters; transition edge sensors; X-ray spectroscopy AB We have studied crosstalk on our 8x8 transition-edge sensor (TES) x-ray microcalorimeter arrays. The shapes of thermal crosstalk pulses are well reproduced as a convolution of heat input from the source pixel and decay in the receiver pixel. We have measured the amount of thermal crosstalk as a function of distance between the source and receiver pixels. Using the results, we have estimated the degradation of energy resolution due to the thermal crosstalk as a function of count rate to determine the level of thermal crosstalk that is needed to satisfy the requirements of NASA's Constellation-X mission. C1 [Iyomoto, N.; Bandler, S. R.; Brekosky, R. P.; Brown, A. -D.; Chervenak, J. A.; Figueroa-Feliciano, E.; Finkbeiner, F. M.; Kelley, R. L.; Kilbourne, C. A.; Porter, F. S.; Sadleir, J. E.; Smith, S. J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Iyomoto, N (reprint author), NASA, Goddard Space Flight Ctr, Code 662, Greenbelt, MD 20771 USA. EM Naoko.Iyomoto@nasa.gov RI Brown, Ari/B-1693-2008; Bandler, Simon/A-6258-2010; Smith, Stephen/B-1256-2008; Porter, Frederick/D-3501-2012; Kelley, Richard/K-4474-2012 OI Bandler, Simon/0000-0002-5112-8106; Smith, Stephen/0000-0003-4096-4675; Porter, Frederick/0000-0002-6374-1119; NR 4 TC 4 Z9 4 U1 0 U2 0 PU SPRINGER/PLENUM PUBLISHERS PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0022-2291 J9 J LOW TEMP PHYS JI J. Low Temp. Phys. PD APR PY 2008 VL 151 IS 1-2 BP 506 EP 512 DI 10.1007/s10909-007-9682-5 PG 7 WC Physics, Applied; Physics, Condensed Matter SC Physics GA 270CP UT WOS:000253697900082 ER PT J AU Mazin, BA Eckart, ME Bumble, B Golwala, S Day, PK Gao, J Zmuidzinas, J AF Mazin, B. A. Eckart, M. E. Bumble, B. Golwala, S. Day, P. K. Gao, J. Zmuidzinas, J. TI Optical/UV and x-ray microwave kinetic inductance strip detectors SO JOURNAL OF LOW TEMPERATURE PHYSICS LA English DT Article; Proceedings Paper CT 12th International Workshop on Low Temperature Detectors CY JUL 22-27, 2007 CL Paris, FRANCE DE microwave; kinetic; inductance; detector; MKID; LTD ID SPECTROPHOTOMETER; ENERGY AB Microwave Kinetic Inductance Detectors (MKIDs) are superconducting detectors that sense the change in the surface impedance of a thin superconducting film when Cooper Pairs are broken by using a high quality factor resonant circuit. We are developing strip detectors that have aluminum MKID sensors on both ends of a rectangular tantalum strip. These devices can provide one dimensional spatial imaging with high quantum efficiency, energy resolution, and microsecond time resolution for single photons from the IR to the X-ray. We have demonstrated X-ray strip detectors with an energy resolution of 62 eV at 6 keV, and hope to improve this substantially. We will also report on our progress towards optical arrays for a planned camera for the Palomar 200 '' telescope. C1 [Mazin, B. A.; Eckart, M. E.; Bumble, B.; Golwala, S.; Day, P. K.; Gao, J.; Zmuidzinas, J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Mazin, BA (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM ben.mazin@jpl.nasa.gov RI Mazin, Ben/B-8704-2011 OI Mazin, Ben/0000-0003-0526-1114 NR 10 TC 17 Z9 17 U1 0 U2 1 PU SPRINGER/PLENUM PUBLISHERS PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0022-2291 J9 J LOW TEMP PHYS JI J. Low Temp. Phys. PD APR PY 2008 VL 151 IS 1-2 BP 537 EP 543 DI 10.1007/s10909-007-9686-1 PG 7 WC Physics, Applied; Physics, Condensed Matter SC Physics GA 270CP UT WOS:000253697900087 ER PT J AU Golwala, S Gao, J Moore, D Mazin, B Eckart, M Bumble, B Day, P LeDuc, HG Zmuidzinas, J AF Golwala, S. Gao, J. Moore, D. Mazin, B. Eckart, M. Bumble, B. Day, P. LeDuc, H. G. Zmuidzinas, J. TI A WIMP dark matter detector using MKIDs SO JOURNAL OF LOW TEMPERATURE PHYSICS LA English DT Article; Proceedings Paper CT 12th International Workshop on Low Temperature Detectors CY JUL 22-27, 2007 CL Paris, FRANCE DE WIMP detectors; dark matter detectors; microwave kinetic inductance detectors; phonon-mediated detectors; strip detectors; position-sensitive detectors; nuclear-recoil discrimination ID DYNAMICS; ARRAYS AB We are pursuing the development of a phonon- and ionization-mediated WIMP dark matter detector employing microwave kinetic inductance detectors (MKIDs) in the phonon-sensing channel. Prospective advantages over existing detectors include: improved reconstruction of the phonon signal and event position; simplified readout wiring and cold electronics; and simplified and more reliable fabrication. We have modeled a simple design using available MKID sensitivity data and anticipate energy resolution as good as existing phonon-mediated detectors and improved position reconstruction. We are doing preparatory experimental work by fabricating strip absorber architectures. Measurements of diffusion length, trapping efficiency, and MKID sensitivity with these devices will enable us to design a 1 cm(2) x 2 mm prototype device to demonstrate phonon energy resolution and position reconstruction. C1 [Golwala, S.; Gao, J.; Moore, D.; Eckart, M.; Zmuidzinas, J.] CALTECH, Div Phys Math & Astron, Pasadena, CA 91125 USA. [Mazin, B.; Bumble, B.; Day, P.; LeDuc, H. G.; Zmuidzinas, J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Golwala, S (reprint author), CALTECH, Div Phys Math & Astron, Pasadena, CA 91125 USA. EM golwala@caltech.edu RI Mazin, Ben/B-8704-2011 OI Mazin, Ben/0000-0003-0526-1114 NR 15 TC 11 Z9 11 U1 0 U2 0 PU SPRINGER/PLENUM PUBLISHERS PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0022-2291 J9 J LOW TEMP PHYS JI J. Low Temp. Phys. PD APR PY 2008 VL 151 IS 1-2 BP 550 EP 556 DI 10.1007/s10909-007-9687-0 PG 7 WC Physics, Applied; Physics, Condensed Matter SC Physics GA 270CP UT WOS:000253697900089 ER PT J AU Gao, J Zmuidzinas, J Vayonakis, A Day, P Mazin, B Leduc, H AF Gao, J. Zmuidzinas, J. Vayonakis, A. Day, P. Mazin, B. Leduc, H. TI Equivalence of the effects on the complex conductivity of superconductor due to temperature change and external pair breaking SO JOURNAL OF LOW TEMPERATURE PHYSICS LA English DT Article; Proceedings Paper CT 12th International Workshop on Low Temperature Detectors CY JUL 22-27, 2007 CL Paris, FRANCE DE complex conductivity; kinetic inductance detector AB The responsivity of microwave kinetic inductance detector (MKID) is related to the derivative of the complex conductivity sigma with respect to the quasiparticle density n(qp). For thermal quasiparticles, this derivative d sigma/dn(qp) can be evaluated from s( T) and nqp( T) given by the Marttis-Bardeen theory (Phys. Rev. 14: 412, 1958). For excess quasiparticles due to external pair breaking, d sigma/dn(qp) can be evaluated by introducing an effective chemical potential mu* into the Marttis-Bardeens theory, as did by Owen and Scalapino ( Phys. Rev. Lett. 28: 1559, 1972). In this paper, we derive the expressions of d sigma/dn(qp) for both thermal and excess quasiparticles and show that they are approximately equal within the temperature and frequency range MKIDs operate. This equivalence validates the method of using bath temperature sweep to calibrate the responsivity of MKIDs. Response curves of an antenna-coupled submm MKID to bath temperature sweep and blackbody source temperature sweep are compared which demonstrates this equivalence. C1 [Gao, J.; Zmuidzinas, J.; Vayonakis, A.] CALTECH, Dept Phys, Pasadena, CA 91125 USA. [Day, P.; Mazin, B.; Leduc, H.] Jet Propuls Lab, Pasadena, CA 91109 USA. RP Gao, J (reprint author), CALTECH, Dept Phys, Pasadena, CA 91125 USA. EM jiansong@caltech.edu RI Mazin, Ben/B-8704-2011 OI Mazin, Ben/0000-0003-0526-1114 NR 8 TC 27 Z9 27 U1 1 U2 7 PU SPRINGER/PLENUM PUBLISHERS PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0022-2291 J9 J LOW TEMP PHYS JI J. Low Temp. Phys. PD APR PY 2008 VL 151 IS 1-2 BP 557 EP 563 DI 10.1007/s10909-007-9688-z PG 7 WC Physics, Applied; Physics, Condensed Matter SC Physics GA 270CP UT WOS:000253697900090 ER PT J AU Zak, M AF Zak, Michail TI Quantum-inspired maximizer SO JOURNAL OF MATHEMATICAL PHYSICS LA English DT Article ID DYNAMICS AB The objective of this paper is to create a new kind of dynamical systems-a quantum-classical hybrid-that would preserve superposition and entanglement of random solutions while allowing one to measure their state variables by using classical methods. Such an optimal combination of characteristics is a perfect match for quantum-inspired computing. The model is represented by a modified Madelung equation in which the quantum potential is replaced by a different, specially chosen "computational" potential. As a result, the dynamics attains both quantum and classical properties. Similarities and differences of the proposed model with quantum systems are outlined. As an application, an algorithm for the global maximum of an arbitrary integrable function is proposed. The idea of the proposed algorithms is very simple: based on the quantum-inspired maximizer, introduce a positive function to be maximized as the probability density to which the solution is attracted. Then, the larger value of this function will have the higher probability to appear. Special attention is paid to the simulation of integer programming, NP-complete problems and information retrieval. (c) 2008 American Institute of Physics. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Zak, M (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM michail.zak@gmail.com NR 17 TC 7 Z9 7 U1 0 U2 0 PU AMER INST PHYSICS PI MELVILLE PA CIRCULATION & FULFILLMENT DIV, 2 HUNTINGTON QUADRANGLE, STE 1 N O 1, MELVILLE, NY 11747-4501 USA SN 0022-2488 J9 J MATH PHYS JI J. Math. Phys. PD APR PY 2008 VL 49 IS 4 AR 042702 DI 10.1063/1.2908281 PG 15 WC Physics, Mathematical SC Physics GA 295DY UT WOS:000255456400017 ER PT J AU Rothman, LS Martin-Torres, FJ Flaud, JM AF Rothman, Laurence S. Martin-Torres, F. Javier Flaud, Jean-Marie TI Special issue on planetary atmospheres - Preface SO JOURNAL OF QUANTITATIVE SPECTROSCOPY & RADIATIVE TRANSFER LA English DT Editorial Material C1 [Rothman, Laurence S.] Harvard Smithsonian Ctr Astrophys, Atom & Mol Phys Div, Cambridge, MA 02138 USA. [Martin-Torres, F. Javier] AS&M Inc, NASA, Langley Res Ctr, Hampton, VA USA. [Flaud, Jean-Marie] Univ Paris 12, F-94010 Creteil, France. [Flaud, Jean-Marie] Univ Paris 07, LISA, F-75221 Paris, France. [Flaud, Jean-Marie] CNRS, F-75700 Paris, France. RP Rothman, LS (reprint author), Harvard Smithsonian Ctr Astrophys, Atom & Mol Phys Div, MS50,60 Garden St, Cambridge, MA 02138 USA. EM lrothman@cfa.harvard.edu RI Martin-Torres, Francisco Javier/G-6329-2015; OI Martin-Torres, Francisco Javier/0000-0001-6479-2236; Rothman, Laurence/0000-0002-3837-4847 NR 0 TC 4 Z9 4 U1 0 U2 3 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0022-4073 J9 J QUANT SPECTROSC RA JI J. Quant. Spectrosc. Radiat. Transf. PD APR PY 2008 VL 109 IS 6 BP 881 EP 881 DI 10.1016/j.jqsrt.2008.02.002 PG 1 WC Optics; Spectroscopy SC Optics; Spectroscopy GA 292WZ UT WOS:000255298100001 ER PT J AU Villanueva, GL Mumma, MJ Novak, RE Hewagama, T AF Villanueva, Gerommo L. Mumma, Michael J. Novak, Robert E. Hewagama, Tilak TI Discovery of multiple bands of isotopic CO2 in the prime spectral regions used when searching for CH4 and HDO on Mars SO JOURNAL OF QUANTITATIVE SPECTROSCOPY & RADIATIVE TRANSFER LA English DT Article DE carbon dioxide; isotopes; intensities; near infrared; Mars; biomarkers ID ATMOSPHERE AB We present new measurements of vibrational band systems of isotopic carbon dioxide (CO2) with multiple strong lines in the wavelength region 3.3-3.7 mu m. In our ground-based searches for methane (CH4) and other biomarker gases on Mars, we discovered two new vibrational band systems that we identify as the previously unknown v(2) + v(3) band of (OCO)-O-16-C-12-O-18 and the 2v(1) band of the rare isotope (OCO)-O-16-C-13-O-18. We also extended and provide refined spectroscopic constants for the 2v(1) band of (OCO)-O-16-C-12-O-17, detecting 38 new lines. The newly discovered 2v(1) band of (OCO)-O-16-C-13-O-18 at 3.7 mu m and the 2v(1) band of (OCO)-O-16-C-12-O-17 at 3.6 mu m extend over the prime spectral region used when searching for deuterated water (HDO) and formaldehyde (H2CO) on Mars. The v(2) + v(3) band of (OCO)-O-16-C-12-O-18 at 3.3 mu m interferes with the v(3) band of CH4 at 3.3 mu m. If unrecognized, even weak bands of CO2 can obscure searches for trace gases on Mars, so it is important to quantify them. Here, we report molecular parameters from the measured line positions that agree well with values calculated from the known energy levels of these isotopologues, and we provide absolute band strengths for each system. (C) 2008 Elsevier Ltd. All rights reserved. C1 [Villanueva, Gerommo L.; Hewagama, Tilak] NASA, Goddard Space Flight Ctr, Solar Syst Explorat Div, Greenbelt, MD 20771 USA. [Novak, Robert E.] Iona Coll, Dept Phys, New Rochelle, NY 10801 USA. [Hewagama, Tilak] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. RP Villanueva, GL (reprint author), NASA, Goddard Space Flight Ctr, Solar Syst Explorat Div, Mailstop 693, Greenbelt, MD 20771 USA. EM geronimo.villanueva@nasa.gov RI Hewagama, T/C-8488-2012; mumma, michael/I-2764-2013 NR 16 TC 18 Z9 18 U1 0 U2 2 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0022-4073 J9 J QUANT SPECTROSC RA JI J. Quant. Spectrosc. Radiat. Transf. PD APR PY 2008 VL 109 IS 6 BP 883 EP 894 DI 10.1016/j.jqsrt.2007.12.016 PG 12 WC Optics; Spectroscopy SC Optics; Spectroscopy GA 292WZ UT WOS:000255298100002 ER PT J AU Toth, RA Brown, LR Miller, CE Devi, VM Benner, DC AF Toth, R. A. Brown, L. R. Miller, C. E. Devi, V. Malathy Benner, D. Chris TI Spectroscopic database of CO2 line parameters: 4300-7000 cm(-1) SO JOURNAL OF QUANTITATIVE SPECTROSCOPY & RADIATIVE TRANSFER LA English DT Article DE near infrared; carbon dioxide; CO2; positions; intensities; self-broadening; air-broadening; Lorentz widths; pressure shifts; database ID CONSTRAINED MULTISPECTRUM ANALYSIS; NEAR-INFRARED SPECTROSCOPY; CARBON-DIOXIDE; SPEED DEPENDENCE; ATMOSPHERIC CO2; ENERGY-LEVELS; INTENSITIES; POSITIONS; BANDS; (CO2)-C-12-O-16 AB A new spectroscopic database for carbon dioxide in the near infrared is presented to support remote sensing of the terrestrial planets (Mars, Venus and the Earth). The compilation contains over 28,500 transitions of 210 bands from 4300 to 7000 cm(-1) and involves nine isotopologues: (OCO)-O-16-C-12-O-16 (626), (OCO)-O-16-C-13-O-16 (636), (OCO)-O-16-C-12-O-18 (628), (OCO)-O-16-C-12-O-17 (627), (OCO)-O-16-C-13-O-18 (638), (OCO)-O-16-C-13-O-17 (637), (OCO)-O-18-C-12-O-18 (828), (OCO)-O-17-C-12-O-18 (728) and (OCO)-O-18-C-13-O-18 (838). Calculated line positions, line intensities, Lorentz half-width and pressure-induced shift coefficients for self- and air-broadening are taken from our recent measurements and are presented for the Voigt molecular line shape. The database includes line intensities for 108 bands measured using the McMath-Pierce Fourier transform spectrometer located on Kitt Peak, Arizona. The available broadening parameters (half-widths and pressure-induced shifts) of (OCO)-O-16-C-12-O-16 are applied to all isotopologues. Broadening coefficients are computed using empirical expressions that have been fitted to the experimental data. There are limited data for the temperature dependence of widths and so no improvement has been made for those parameters. The line intensities included in the catalog vary from 4 x 10(-30) to 1.29 x 10(-21) cm(-1)/(molecule cm(-2)) at 296 K. The total integrated intensity for this spectral interval is 5.9559 x 10(-20) cm(-1)/(molecule cm(-2)) at 296 K. (C) 2008 Elsevier Ltd. All rights reserved. C1 [Toth, R. A.; Brown, L. R.; Miller, C. E.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Devi, V. Malathy; Benner, D. Chris] Coll William & Mary, Williamsburg, VA 23187 USA. RP Toth, RA (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM ratoth@jpl.nasa.gov NR 55 TC 79 Z9 79 U1 1 U2 18 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0022-4073 J9 J QUANT SPECTROSC RA JI J. Quant. Spectrosc. Radiat. Transf. PD APR PY 2008 VL 109 IS 6 BP 906 EP 921 DI 10.1016/j.jqsrt.2007.12.004 PG 16 WC Optics; Spectroscopy SC Optics; Spectroscopy GA 292WZ UT WOS:000255298100004 ER PT J AU Smith, MAH Rinsland, CP Blake, TA Sams, RL Benner, DC Devi, VM AF Smith, M. A. H. Rinsland, C. P. Blake, T. A. Sams, R. L. Benner, D. Chris Devi, V. Malathy TI Low-temperature measurements of HCN broadened by N-2 in the 14-mu m spectral region SO JOURNAL OF QUANTITATIVE SPECTROSCOPY & RADIATIVE TRANSFER LA English DT Article DE HCN; Lorentz N-2-broadening; N-2 pressure-induced shifts; relaxation matrix elements; speed dependence; temperature dependence; line mixing ID DIODE-LASER MEASUREMENTS; MOLECULAR SPECTROSCOPIC DATABASE; MULTISPECTRUM ANALYSIS; SHIFT COEFFICIENTS; TITANS ATMOSPHERE; NU(2) BAND; V(1) BAND; NU-2 BAND; V(2) BAND; PART II AB Half-width and pressure-induced shift coefficients; the temperature-dependence exponents of the half-widths and the temperature-dependence coefficients of pressure-induced shifts have been measured for N-2-broadened transitions in the v(2) band of HCN. Line positions and intensities were also determined. A total of 34 laboratory absorption spectra, recorded at 0.002-0.005 cm(-1) resolution with two different Fourier transform spectrometers, were used in the determination of the spectral line parameters. The total pressures of the HCN-N-2 samples ranged from less than 1 torr up to nearly 1 atm, and temperatures were between 211 and 300 K. A multispectrum nonlinear least-squares fitting technique employing a modified Voigt line profile, including speed dependence and line mixing via the off-diagonal relaxation matrix formulation, was used in the analysis. Speed-dependence parameters were determined in the P and R branches of the v(2) band of (HCN)-C-12-N-14, and in the v(2) Q branches of (HCN)-C-12-N-14 and (HCN)-C-13-N-14 the off-diagonal relaxation matrix elements that characterize line mixing were included in the analysis to fit the data. Present results are compared with previous measurements reported in the literature. (C) 2007 Published by Elsevier Ltd. C1 [Smith, M. A. H.; Rinsland, C. P.] NASA, Langley Res Ctr, Sci Directorate, Hampton, VA 23681 USA. [Blake, T. A.; Sams, R. L.] Pacific NW Natl Lab, Richland, WA 99352 USA. [Benner, D. Chris; Devi, V. Malathy] Coll William & Mary, Dept Phys, Williamsburg, VA 23187 USA. RP Smith, MAH (reprint author), NASA, Langley Res Ctr, Sci Directorate, MS 401A, Hampton, VA 23681 USA. EM Mary.Ann.H.Smith@nasa.gov NR 45 TC 2 Z9 2 U1 2 U2 3 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0022-4073 J9 J QUANT SPECTROSC RA JI J. Quant. Spectrosc. Radiat. Transf. PD APR PY 2008 VL 109 IS 6 BP 922 EP 951 DI 10.1016/j.jqsrt.2007.12.017 PG 30 WC Optics; Spectroscopy SC Optics; Spectroscopy GA 292WZ UT WOS:000255298100005 ER PT J AU Rinsland, CP Devi, VM Benner, DC Blake, TA Sams, RL Brown, LR Kleiner, I Dehayem-Kamadjeu, A Muller, HSP Gamache, RR Niles, DL Masiello, T AF Rinsland, C. P. Devi, V. Malathy Benner, D. Chris Blake, T. A. Sams, R. L. Brown, L. R. Kleiner, I. Dehayem-Kamadjeu, A. Mueller, H. S. P. Gamache, R. R. Niles, D. L. Masiello, T. TI Multispectrum analysis of the v(4) band of CH3CN: Positions, intensities, self- and N-2-broadening, and pressure-induced shifts SO JOURNAL OF QUANTITATIVE SPECTROSCOPY & RADIATIVE TRANSFER LA English DT Article DE CH3CN; atmosphere of Titan; remote sounding; Fourier transform infrared (FTIR) spectroscopy; pressure broadening; pressure-induced shifts; spectral line shape; partition function; transmission and scattering of radiation ID METHYL CYANIDE; SPECTROSCOPIC DATABASE; MOLECULAR-SPECTROSCOPY; ROTATIONAL SPECTRUM; COLOGNE DATABASE; LIMB SOUNDER; LINE; METHYLCYANIDE; FREQUENCIES; STATES AB A multispectrum nonlinear least-squares fitting technique was applied to measure accurate zero-pressure line center positions, Lorentz self- and nitrogen (N-2)-broadened half-width coefficients, and self- and N-2-pressure-induced shift coefficients for over 700 transitions in the parallel v(4) band of CH3CN near 920 cm(-1). Fifteen high-resolution (0.0016 cm(-1)) laboratory absorption spectra of pure and N-2-broadened CH3CN recorded at room temperature using the Bruker IFS 125HR Fourier transform spectrometer located at the Pacific Northwest National Laboratory (PNNL) in Richland, Washington, USA, were analyzed simultaneously assuming standard Voigt line shapes. Short spectral intervals containing manifolds of transitions from the same value of J were fitted together. In all, high-precision line parameters were obtained for P(44)-P(3)(-) and R(0)-R(46) manifolds. As part of the analysis, quantum assignments were extended, and the total internal partition function sum was calculated for four isotopologs: (CH3CN)-C-12-C-12, (CH3CN)-C-13-C-12, (CH3CN)-C-12-C-13, and (CH3CN)-C-13-C-13. Measurements of N-2 broadening, self-broadening, N-2-shift, and self-shift coefficients for transitions with J up to 48 and K up to 12 were measured for the first time in the mid-infrared. Self-broadened half-width coefficients were found to be very large (up to similar to 2cm(-1) atm(-1) at 296K). Ratios of self-broadened half-width coefficients to N-2-broadened half-width coefficients show a compact distribution with rotational quantum number in both the P and R branches that range from similar to 4.5 to 14 with maxima near vertical bar m vertical bar = 24, where m = -J '', J '', and J '' + 1 for P, Q and R lines, respectively. Pressure-induced shifts for N-2 are small (few exceed + 0.006 cm(-1) atm(-1) at 294 K) and are both positive and negative. In contrast, self-shift coefficients are large (maxima of about +/- 0.08 cm(-1) atm(-1) at 294 K) and are both positive and negative as a function of rotational quantum numbers. The present measured half-widths and pressure shifts in v(4) were compared with corresponding measurements of rotational transitions. (C) 2007 Elsevier Ltd. All rights reserved. C1 [Rinsland, C. P.] NASA, Langley Res Ctr, Hampton, VA 23681 USA. [Devi, V. Malathy; Benner, D. Chris] Coll William & Mary, Dept Phys, Williamsburg, VA 23187 USA. [Blake, T. A.; Sams, R. L.; Masiello, T.] Pacific NW Natl Lab, Richland, WA 99352 USA. [Brown, L. R.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Kleiner, I.; Dehayem-Kamadjeu, A.] Univ Paris 07, Lab Interuniv Syst Atmospher, F-94010 Creteil, France. [Kleiner, I.; Dehayem-Kamadjeu, A.] Univ Paris 12, F-94010 Creteil, France. [Kleiner, I.; Dehayem-Kamadjeu, A.] CNRS, F-94010 Creteil, France. [Mueller, H. S. P.] Univ Cologne, Inst Phys 1, D-50937 Cologne, Germany. [Gamache, R. R.; Niles, D. L.] Univ Massachusetts, Dept Environm Earth & Atmospher Sci, Lowell, MA 01854 USA. RP Rinsland, CP (reprint author), NASA, Langley Res Ctr, Mail Stop 401A, Hampton, VA 23681 USA. EM curtis.p.rinsland@nasa.gov; Malathy.D.Venkataraman@nasa.gov; dcbenn@wm.edu; ta.blake@pnl.gov; robert.sams@pnl.gov; Linda.R.Brown@jpl.nasa.gov; kleiner@lisa.univ-paris12.fr; dehayem@lisa.univ-paris12.fr; hspm@ph1.uni-koeln.de; Robert_Gamache@uml.edu; dlniles@gmail.com; tony.masiello@nist.gov NR 49 TC 17 Z9 17 U1 0 U2 8 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0022-4073 J9 J QUANT SPECTROSC RA JI J. Quant. Spectrosc. Radiat. Transf. PD APR PY 2008 VL 109 IS 6 BP 974 EP 994 DI 10.1016/j.jqsrt.2007.11.013 PG 21 WC Optics; Spectroscopy SC Optics; Spectroscopy GA 292WZ UT WOS:000255298100008 ER PT J AU Jacquinet-Husson, N Scott, NA Chedina, A Crepeau, L Armante, R Capelle, V Orphal, J Coustenis, A Boonne, C Poulet-Crovisier, N Barbee, A Birk, M Brown, LR Camy-Peyret, C Claveau, C Chance, K Christidis, N Clerbaux, C Coheur, PF Dana, V Daumont, L De Backer-Barilly, MR Di Lonardo, G Flaud, JM Goldman, A Hamdouni, A Hess, M Hurley, MD Jacquemart, D Kleiner, I Kopke, P Mandin, JY Massie, S Mikhailenko, S Nemtchinov, V Nikitin, A Newnham, D Perrin, A Perevalov, VI Pinnock, S Regalia-Jarlot, L Rinsland, CP Rublev, A Schreier, F Schult, L Smith, KM Tashkun, SA Teffo, JL Toth, RA Tyuterev, VG Auwera, JV Varanasi, P Wagner, G AF Jacquinet-Husson, N. Scott, N. A. Chedina, A. Crepeau, L. Armante, R. Capelle, V. Orphal, J. Coustenis, A. Boonne, C. Poulet-Crovisier, N. Barbee, A. Birk, M. Brown, L. R. Camy-Peyret, C. Claveau, C. Chance, K. Christidis, N. Clerbaux, C. Coheur, P. F. Dana, V. Daumont, L. De Backer-Barilly, M. R. Di Lonardo, G. Flaud, J. M. Goldman, A. Hamdouni, A. Hess, M. Hurley, M. D. Jacquemart, D. Kleiner, I. Koepke, P. Mandin, J. Y. Massie, S. Mikhailenko, S. Nemtchinov, V. Nikitin, A. Newnham, D. Perrin, A. Perevalov, V. I. Pinnock, S. Regalia-Jarlot, L. Rinsland, C. P. Rublev, A. Schreier, F. Schult, L. Smith, K. M. Tashkun, S. A. Teffo, J. L. Toth, R. A. Tyuterev, Vl. G. Auwera, J. Vander Varanasi, P. Wagner, G. TI The GEISA spectroscopic database: Current and future archive for Earth and planetary atmosphere studies SO JOURNAL OF QUANTITATIVE SPECTROSCOPY & RADIATIVE TRANSFER LA English DT Review DE GEISA; spectroscopic database; line parameters; cross-sections; atmospheric absorption; atmospheric aerosols; Earth's and planetary atmospheres ID ABSORPTION CROSS-SECTIONS; FOURIER-TRANSFORM SPECTROSCOPY; O-2 HERZBERG BANDS; ROTATIONAL LINE POSITIONS; SENSING REFERENCE DATA; M SPECTRAL REGION; 231-794 NM RANGE; MU-M; WATER-VAPOR; CARBON-DIOXIDE AB The development of Gestion et Etude des Informations Spectroscopiques Atmospheriques (GEISA: Management and Study of Spectroscopic Information) was started over three decades at Laboratoire de Meteorologie Dynamique (LMD) in France. GEISA is a computer accessible spectroscopic database, designed to facilitate accurate forward radiative transfer calculations using a line-by-line and layer-by-layer approach. More than 350 users have been registered for on-line use of the GEISA facilities. The current 2003 edition of GEISA (GEISA-03) is a system comprising three independent sub-databases devoted respectively to: line transition parameters, infrared and ultraviolet/visible absorption cross-sections, microphysical and optical properties of atmospheric aerosols. Currently., GEISA is involved in activities related to the assessment of the capabilities of IASI (Infrared Atmospheric Sounding Interferometer on board of the METOP European satellite) through the GEISA/IASI database derived from GEISA. The GEISA-03 content is presented, placing emphasis on molecular species of interest for Earth and planetary atmosphere studies, with details on the updated 2008 archive underway. A critical assessment on the needs, in terms of molecular parameters archive, related with recent satellite astrophysical missions is made. Detailed information on free online GEISA and GEISA/IASI access is given at http://ara.lmd.polytechnique.fr and http://ether.ipsl.jussieu.fr. (C) 2008 Elsevier Ltd. All rights reserved. C1 [Jacquinet-Husson, N.; Scott, N. A.; Chedina, A.; Crepeau, L.; Armante, R.; Capelle, V.] Ecole Polytech, Inst Pierre Simon Laplace, Meteorol Dynam Lab, F-91128 Palaiseau, France. [Orphal, J.; Flaud, J. M.; Kleiner, I.; Perrin, A.] Fac Sci & Technol, Lab Interuniv Syst Atmospher, F-94010 Creteil, France. [Coustenis, A.] Observ Paris, Lab Etud Spatiales & Instrumentat Astrophys, F-92195 Meudon, France. [Barbee, A.; Daumont, L.; De Backer-Barilly, M. R.; Hamdouni, A.; Regalia-Jarlot, L.; Tyuterev, Vl. G.] Univ Reims, Grp Spectrometrie Mol & Atmospher, F-51062 Reims, France. [Birk, M.; Schreier, F.; Wagner, G.] DLR, Remote Sensing Technol Inst, D-82234 Oberpfaffenhofen, Wessling, Germany. [Brown, L. R.; Toth, R. A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Camy-Peyret, C.; Claveau, C.; Dana, V.; Mandin, J. Y.; Teffo, J. L.] Univ Paris 06, Lab Phys Mol Atmosphere & Astrophys, F-94200 Ivry, France. [Chance, K.; Clerbaux, C.; Coheur, P. F.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Christidis, N.; Pinnock, S.] Univ Reading, Dept Meteorol, Reading RG6 2AU, Berks, England. [Clerbaux, C.] Univ Paris 06, Inst Pierre Simon Laplace, Serv Aeron, F-75252 Paris, France. [Coheur, P. F.; Auwera, J. Vander] Univ Libre Bruxelles, Serv Chim Quant & Photophys, B-1050 Brussels, Belgium. [Di Lonardo, G.] Univ Bologna, Dipartimento Chim Fis & Inorgan, I-40136 Bologna, Italy. [Goldman, A.] Univ Denver, Dept Phys, Denver, CO 80208 USA. [Hurley, M. D.] Ford Res Lab, Dearborn, MI 48124 USA. [Jacquemart, D.] Univ Paris 06, Lab Dynam Interact & React, F-75252 Paris, France. [Koepke, P.] Univ Munich, Inst Meteorol, D-80333 Munich, Germany. [Massie, S.] Natl Ctr Atmospher Res, Boulder, CO 80307 USA. [Mikhailenko, S.; Nikitin, A.; Perevalov, V. I.; Tashkun, S. A.] Russian Acad Sci, Inst Atmospher Opt, Lab Theoret Spect, Tomsk 634055, Russia. [Nemtchinov, V.; Varanasi, P.] SUNY Stony Brook, Stony Brook, NY 11794 USA. [Newnham, D.; Smith, K. M.] Rutherford Appleton Lab, Didcot OX11 0QX, Oxon, England. [Rinsland, C. P.] NASA, Langley Res Ctr, Sci Directorate, Hampton, VA 23681 USA. [Rublev, A.] Russian Res Ctr, Inst Mol Phys, Kurchatov Inst, Moscow 123183, Russia. [Schult, L.] Max Planck Inst Meteorol, D-20146 Hamburg, Germany. RP Jacquinet-Husson, N (reprint author), Ecole Polytech, Inst Pierre Simon Laplace, Meteorol Dynam Lab, Route Dept 36, F-91128 Palaiseau, France. EM jacquinet@lmd.polytechnique.fr RI Orphal, Johannes/A-8667-2012; Nikitin, Andrei/K-2624-2013; Tashkun, Sergey/E-8682-2014; clerbaux, cathy/I-5478-2013; OI Orphal, Johannes/0000-0002-1943-4496; Nikitin, Andrei/0000-0002-4280-4096; Chance, Kelly/0000-0002-7339-7577 NR 104 TC 126 Z9 127 U1 1 U2 21 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0022-4073 EI 1879-1352 J9 J QUANT SPECTROSC RA JI J. Quant. Spectrosc. Radiat. Transf. PD APR PY 2008 VL 109 IS 6 BP 1043 EP 1059 DI 10.1016/j.jqsrt.2007.12.015 PG 17 WC Optics; Spectroscopy SC Optics; Spectroscopy GA 292WZ UT WOS:000255298100013 ER PT J AU Kratz, DP AF Kratz, David P. TI The sensitivity of radiative transfer calculations to the changes in the HITRAN database from 1982 to 2004 SO JOURNAL OF QUANTITATIVE SPECTROSCOPY & RADIATIVE TRANSFER LA English DT Article DE HITRAN database; line parameters; line-by-line calculation; correlated k-distribution; infrared; radiances; fluxes; radiative forcings ID MOLECULAR SPECTROSCOPIC DATABASE; K-DISTRIBUTION METHOD; WATER-VAPOR; CERES WINDOW; Q-BRANCHES; ABSORPTION; EDITION; CLOUDS; COMPILATION; ATMOSPHERES AB Over the last quarter century, improvements in the determination of the spectroscopic characteristics of the infrared-active trace species have enhanced our ability to retrieve quantitative distributions of temperatures, clouds, and abundances for various trace species within the Earth's atmosphere. These improvements have also allowed for refinements in the estimates of climatic effects attributed to changes in the Earth's atmospheric composition. Modeling efforts, however, have frequently experienced significant delays in assimilating improved spectroscopic information. Such is the case for highly parameterized models, where considerable effort is typically required to incorporate any revisions. Thus, a line-by-line radiative transfer model has been used to investigate the magnitude of the effects resulting from modifications to the spectroscopic information. Calculations from this line-by-line model have demonstrated that recent modifications to the HITRAN (High Resolution Transmission) line parameters, the continuum formulation, and the CO2 line-mixing formulation can significantly affect the interpretation of the high spectral resolution radiance and brightness temperature retrievals. For certain moderate-resolution satellite remote sensing channels, modifications to these spectroscopic parameters and formulations have shown the capacity to induce changes in the calculated radiances equivalent to brightness temperature differences of 1-2K. Model calculations have further shown that modifications of the spectroscopic characteristics tend to have a modest effect on the determination of spectrally integrated radiances, fluxes, and radiative forcing estimates, with the largest differences being of order 1 W m(-2) for the total thermal infrared fluxes, and of order 2-3% of the calculated radiative forcing at the tropopause attributed to the combined doubling of CO2, N2O, and CH4. The results from this investigation are intended to function as a guide to differentiate between cases where older parameterizations provide acceptable results, within specified accuracy bounds, and cases where upgrades to the latest spectroscopic database are necessary. Published by Elsevier Ltd. C1 NASA, Langley Res Ctr, Climate Sci Branch, Hampton, VA 23681 USA. RP Kratz, DP (reprint author), NASA, Langley Res Ctr, Climate Sci Branch, Hampton, VA 23681 USA. EM david.p.kratz@nasa.gov NR 40 TC 15 Z9 17 U1 1 U2 3 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0022-4073 EI 1879-1352 J9 J QUANT SPECTROSC RA JI J. Quant. Spectrosc. Radiat. Transf. PD APR PY 2008 VL 109 IS 6 BP 1060 EP 1080 DI 10.1016/j.jqsrt.2007.10.010 PG 21 WC Optics; Spectroscopy SC Optics; Spectroscopy GA 292WZ UT WOS:000255298100014 ER PT J AU Hewagama, T Goldstein, J Livengood, TA Buhl, D Espenak, F Fast, K Kostiuk, T Schmulling, F AF Hewagama, T. Goldstein, J. Livengood, T. A. Buhl, D. Espenak, F. Fast, K. Kostiuk, Th. Schmuelling, F. TI Beam integrated high-resolution infrared spectra: Accurate modeling of thermal emission from extended clear atmospheres SO JOURNAL OF QUANTITATIVE SPECTROSCOPY & RADIATIVE TRANSFER LA English DT Article DE radiative transfer; beam integration; spectroscopy; infrared; atmospheres ID SPECTROSCOPIC DATABASE; TEMPERATURE; TRANSMITTANCE; ABUNDANCE; ETHANE AB We describe a technique for analysis of high resolution thermal IR spectra measured with a finite beam (field of view) on the target planetary atmosphere. The model developed allows a beam integrated radiative transfer calculation over the varying line-of-sight velocity, temperature, and species abundance distributed over the field of view, thus recovering information on atmospheric composition, dynamics, and thermal structure. The modeling procedure is comprises four primary aspects: segmentation of the projected observational beam to a grid of beam elements; determining the geometrical properties of the planetary atmospheric region associated with each beam element; calculating the spectrum emergent from the top of the atmosphere of each element; and weighting the ensemble of spectra with the characteristic observational beam response profile and accumulating the contributions. This prescription results in a beam integrated spectrum-a more accurate representation of fully resolved IR rotation-vibration molecular spectra of planetary atmospheres observed with finite aperture telescopes. The method is implemented as a numerical code appropriate for modeling the spectroscopic observations. This paper describes the basic formalism for beam integrated radiation transfer of planetary atmospheres, discusses the salient points of the modeling process, and quantifies limitations. Application of this technique will be illustrated using high resolution atmospheric molecular spectral line measurements of Titan obtained by infrared heterodyne spectroscopy to extract zonal wind field, temperature and C2H6 abundance. (C) 2007 Elsevier Ltd. All rights reserved. C1 [Hewagama, T.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Goldstein, J.; Livengood, T. A.] Natl Ctr Earth & Space Sci Educ, Columbia, MD 21044 USA. [Hewagama, T.; Livengood, T. A.; Buhl, D.; Espenak, F.; Fast, K.; Kostiuk, Th.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Schmuelling, F.] Univ Cologne, D-5000 Cologne 41, Germany. RP Hewagama, T (reprint author), Univ Maryland, Dept Astron, College Pk, MD 20742 USA. EM tilak@cuzco.gsfc.nasa.gov RI Livengood, Timothy/C-8512-2012; Hewagama, T/C-8488-2012; Kostiuk, Theodor/A-3077-2014 NR 36 TC 6 Z9 6 U1 0 U2 1 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0022-4073 J9 J QUANT SPECTROSC RA JI J. Quant. Spectrosc. Radiat. Transf. PD APR PY 2008 VL 109 IS 6 BP 1081 EP 1097 DI 10.1016/j.jqsrt.2007.12.022 PG 17 WC Optics; Spectroscopy SC Optics; Spectroscopy GA 292WZ UT WOS:000255298100015 ER PT J AU Ustinov, EA AF Ustinov, Eugene A. TI Linearization of radiative heating and cooling rates for the case of non-scattering planetary atmospheres SO JOURNAL OF QUANTITATIVE SPECTROSCOPY & RADIATIVE TRANSFER LA English DT Article DE radiative transfer; sensitivity analysis; heating and cooling rates ID WEIGHTING FUNCTIONS; ADJOINT AB Rates of radiative heating and cooling of the non-scattering planetary atmosphere and scattering underlying surface are analytically linearized with respect to the atmospheric and surface parameters. Resulting expressions for sensitivities of radiative heating and cooling rates are used to formulate the linearized ID radiative model of atmospheric dynamics which directly incorporates the relevant linearized atmospheric and surface parameters. Applications to more sophisticated models of atmospheric dynamics, as well as extension to the case of presence of atmospheric scattering, are briefly discussed. (C) 2007 Elsevier Ltd. All rights reserved. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Ustinov, EA (reprint author), CALTECH, Jet Prop Lab, Mail Stop 169-237,4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM Eugene.A.Ustinov@jpl.nasa.gov RI Ustinov, Eugene/D-1350-2015 OI Ustinov, Eugene/0000-0003-0227-4286 NR 9 TC 0 Z9 0 U1 0 U2 1 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0022-4073 J9 J QUANT SPECTROSC RA JI J. Quant. Spectrosc. Radiat. Transf. PD APR PY 2008 VL 109 IS 6 BP 1098 EP 1117 DI 10.1016/j.jqsrt.2007.12.012 PG 20 WC Optics; Spectroscopy SC Optics; Spectroscopy GA 292WZ UT WOS:000255298100016 ER PT J AU Irwin, PGJ Teanby, NA de Kok, R Fletcher, LN Howett, CJA Tsang, CCC Wilson, CF Calcutt, SB Nixon, CA Parrish, PD AF Irwin, P. G. J. Teanby, N. A. de Kok, R. Fletcher, L. N. Howett, C. J. A. Tsang, C. C. C. Wilson, C. F. Calcutt, S. B. Nixon, C. A. Parrish, P. D. TI The NEMESIS planetary atmosphere radiative transfer and retrieval tool SO JOURNAL OF QUANTITATIVE SPECTROSCOPY & RADIATIVE TRANSFER LA English DT Article DE retrievals; radiative transfer; correlated-k ID MULTIPLE-SCATTERING; SPECTROSCOPIC DATABASE; LATITUDINAL VARIATIONS; TITANS STRATOSPHERE; ABSORPTION-SPECTRA; CASSINI CIRS; PARAMETERS; PHOSPHINE; AMMONIA; CM(-1) AB With the exception of in situ atmospheric probes, the most useful way to study the atmospheres of other planets is to observe their electromagnetic spectra through remote observations, either from ground-based telescopes or from spacecraft. Atmospheric properties most consistent with these observed spectra are then derived with retrieval models. All retrieval models attempt to extract the maximum amount of atmospheric information from finite sets of data, but while the problem to be solved is fundamentally the same for any planetary atmosphere, until now all such models have been assembled ad hoc to address data from individual missions. In this paper, we describe a new general-purpose retrieval model, Non-linear Optimal Estimator for MultivariatE Spectral analySIS (NEMESIS), which was originally developed to interpret observations of Saturn and Titan from the composite infrared spectrometer on board the NASA Cassini spacecraft. NEMESIS has been constructed to be generally applicable to any planetary atmosphere and can be applied from the visible/near-infrared right out to microwave wavelengths, modelling both reflected sunlight and thermal emission in either scattering or non-scattering conditions. NEMESIS has now been successfully applied to the analysis of data from many planetary missions and also ground-based observations. (C) 2007 Elsevier Ltd. All rights reserved. C1 [Irwin, P. G. J.; Teanby, N. A.; de Kok, R.; Fletcher, L. N.; Howett, C. J. A.; Tsang, C. C. C.; Wilson, C. F.; Calcutt, S. B.] Univ Oxford, Clarendon Lab, Oxford OX1 3PU, England. [Nixon, C. A.] Univ Maryland, NASA, Goddard Space Flight Ctr, Solar Syst Explorat Div, Greenbelt, MD 20771 USA. [Parrish, P. D.] Univ Edinburgh, Sch Geosci, Inst Atmospher & Environm Sci, Edinburgh EH9 3JN, Midlothian, Scotland. RP Irwin, PGJ (reprint author), Univ Oxford, Clarendon Lab, Parks Rd, Oxford OX1 3PU, England. EM irwin@atm.ox.ac.uk RI Fletcher, Leigh/D-6093-2011; Nixon, Conor/A-8531-2009; OI Fletcher, Leigh/0000-0001-5834-9588; Nixon, Conor/0000-0001-9540-9121; Calcutt, Simon/0000-0002-0102-3170; Teanby, Nicholas/0000-0003-3108-5775; Irwin, Patrick/0000-0002-6772-384X NR 27 TC 139 Z9 139 U1 1 U2 6 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0022-4073 J9 J QUANT SPECTROSC RA JI J. Quant. Spectrosc. Radiat. Transf. PD APR PY 2008 VL 109 IS 6 BP 1136 EP 1150 DI 10.1016/j.jqsrt.2007.11.006 PG 15 WC Optics; Spectroscopy SC Optics; Spectroscopy GA 292WZ UT WOS:000255298100018 ER PT J AU Nystuen, JA Amitai, E Anagnostou, EN Anagnostou, MN AF Nystuen, Jeffrey A. Amitai, Eyal Anagnostou, Emmanuel N. Anagnostou, Marios N. TI Spatial averaging of oceanic rainfall variability using underwater sound: Ionian sea rainfall experiment 2004 SO JOURNAL OF THE ACOUSTICAL SOCIETY OF AMERICA LA English DT Article ID NOISE AB An experiment to evaluate the inherent spatial averaging of the underwater acoustic signal from rainfall was conducted in the winter of 2004 in the Ionian Sea southwest of Greece. A mooring with four passive aquatic listeners (PALs) at 60, 200, 1000, and 2000 in was deployed at 36.85 degrees N, 21.52 degrees E. 17 kin west of a dual-polarization X-band coastal radar at Methoni, Greece. The acoustic signal is classified into wind, rain, shipping, and whale categories. It is similar at all depths and rainfall is detected at all depths. A signal that is consistent with the clicking of deep-diving beaked whales is present 2% of the time, although there was no visual confirmation of whale presence. Co-detection of rainfall with the radar verifies that the acoustic detection of rainfall is excellent. Once detection is made, the correlation between acoustic and radar rainfall rates is high. Spatial averaging of the radar rainfall rates in concentric circles over the mooring verifies the larger inherent spatial averaging of the rainfall signal with recording depth. For the PAL at 2000 in, the maximum correlation was at 3-4 kin, suggesting a listening area for the acoustic rainfall measurement of roughly 30-50 km(2). (C) 2008 Acoustical Society of America. C1 [Nystuen, Jeffrey A.] Univ Washington, Appl Phys Lab, Seattle, WA 98105 USA. [Amitai, Eyal] George Mason Univ, Ctr Earth Observing & Space Res, Fairfax, VA 22030 USA. [Amitai, Eyal] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Anagnostou, Emmanuel N.; Anagnostou, Marios N.] Univ Connecticut, Dept Civil & Environm Engn, Storrs, CT 06269 USA. RP Nystuen, JA (reprint author), Univ Washington, Appl Phys Lab, 1013 NE 40th St, Seattle, WA 98105 USA. EM nystuen@apl.washington.edu NR 12 TC 9 Z9 11 U1 0 U2 5 PU ACOUSTICAL SOC AMER AMER INST PHYSICS PI MELVILLE PA STE 1 NO 1, 2 HUNTINGTON QUADRANGLE, MELVILLE, NY 11747-4502 USA SN 0001-4966 J9 J ACOUST SOC AM JI J. Acoust. Soc. Am. PD APR PY 2008 VL 123 IS 4 BP 1952 EP 1962 DI 10.1121/1.2871485 PG 11 WC Acoustics; Audiology & Speech-Language Pathology SC Acoustics; Audiology & Speech-Language Pathology GA 289HD UT WOS:000255044700017 PM 18397003 ER PT J AU Wilson, PS Reed, AH Wood, WT Roy, RA AF Wilson, Preston S. Reed, Allen H. Wood, Warren T. Roy, Ronald A. TI The low-frequency sound speed of fluid-like gas-bearing sediments SO JOURNAL OF THE ACOUSTICAL SOCIETY OF AMERICA LA English DT Letter ID ACOUSTIC PROPAGATION; WAVE-PROPAGATION; POROUS-MEDIA; IN-SITU; BUBBLES; LIQUID; PREDICTIONS; SCATTERING; MIXTURE; MODEL AB The low-frequency sound speed in a fluid-like kaolinite sediment containing air bubbles was measured using an acoustic resonator technique and found to be 114 m/s with negligible dispersion between 100 and 400 Hz. The sediment's void fraction and bubble size distribution was determined from volumetric images obtained from x-ray computed tomography scans. A simplified version of Wood's effective medium model, which is dependent only upon the ambient pressure, the void fraction, the sediment's bulk mass density, and the assumption that all the bubbles are smaller than resonance size at the highest frequency of interest, described the measured sound speed. (C) 2008 Acoustical Society of America. C1 [Wilson, Preston S.] Univ Texas Austin, Appl Res Labs, Austin, TX 78713 USA. [Wilson, Preston S.] Univ Texas Austin, Dept Mech Engn, Austin, TX 78712 USA. [Reed, Allen H.; Wood, Warren T.] USN, Res Lab, Stennis Space Ctr, Marine GeoSci Div, Stennis Space Ctr, MS 39529 USA. [Roy, Ronald A.] Boston Univ, Dept Aerosp & Mech Engn, Boston, MA 02215 USA. RP Wilson, PS (reprint author), Univ Texas Austin, Appl Res Labs, POB 8029, Austin, TX 78713 USA. EM pswilson@mail.utexas.edu; allen.reed@nrlssc.navy.mil; warren.wood@nrlssc.navy.mil; ronroy@bu.edu OI Roy, Ronald/0000-0001-6394-5667 NR 18 TC 4 Z9 4 U1 1 U2 5 PU ACOUSTICAL SOC AMER AMER INST PHYSICS PI MELVILLE PA STE 1 NO 1, 2 HUNTINGTON QUADRANGLE, MELVILLE, NY 11747-4502 USA SN 0001-4966 J9 J ACOUST SOC AM JI J. Acoust. Soc. Am. PD APR PY 2008 VL 123 IS 4 BP EL99 EP EL104 DI 10.1121/1.2884081 PG 6 WC Acoustics; Audiology & Speech-Language Pathology SC Acoustics; Audiology & Speech-Language Pathology GA 289HD UT WOS:000255044700071 PM 18396928 ER PT J AU Burnett, J Smith, SM Pickens, S Aung, K Dyer, CB AF Burnett, J. Smith, S. M. Pickens, S. Aung, K. Dyer, C. B. TI Vitamin D Deficiency and physical performance in vulnerable elders who self-neglect SO JOURNAL OF THE AMERICAN GERIATRICS SOCIETY LA English DT Meeting Abstract CT Annual Meeting of the American-Geriatrics-Society CY APR 30-MAY 04, 2008 CL Washington, DC SP Amer Geriatr Soc C1 [Burnett, J.; Pickens, S.; Aung, K.; Dyer, C. B.] Univ Texas Houston, Hlth Sci Ctr, Houston, TX USA. [Smith, S. M.] NASA, Lyndon B Johnson Space Ctr, Human Adapt & Countermeasures Div, Houston, TX 77058 USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU BLACKWELL PUBLISHING PI OXFORD PA 9600 GARSINGTON RD, OXFORD OX4 2DQ, OXON, ENGLAND SN 0002-8614 J9 J AM GERIATR SOC JI J. Am. Geriatr. Soc. PD APR PY 2008 VL 56 IS 4 SU S MA D84 BP S188 EP S188 PG 1 WC Geriatrics & Gerontology; Gerontology SC Geriatrics & Gerontology GA 286IT UT WOS:000254840300544 ER PT J AU Yeo, HS AF Yeo, Hyeonsoo TI Assessment of active controls for rotor performance enhancement SO JOURNAL OF THE AMERICAN HELICOPTER SOCIETY LA English DT Article; Proceedings Paper CT 62nd Annual Forum of the American-Helicopter-Society CY MAY 09-11, 2006 CL Phoenix, AZ ID TRAILING-EDGE FLAPS; HELICOPTER AB A study was conducted to assess the capability of active controls to produce rotor performance improvements. The calculations were conducted using the comprehensive analysis CAMRAD II. The baseline rotor considered was a four-bladed articulated rotor with a VR-12 airfoil. Seven active control concepts were investigated: leading edge slat, variable droop leading edge, oscillatory jet, Gurney flap, individual blade control, active twist, and trailing edge flap. Comparative performance calculations have been conducted for two cases: (1) an airspeed sweep at C-T/sigma = 0.075 to examine rotor lift-to-drag ratio and (2) thrust sweeps at fixed airspeeds to estimate maximum blade loading capability. The individual blade control, active twist, and trailing edge flap concepts improved the rotor lift-to-drag ratio with a 2/rev harmonic control. The remaining four concepts-leading edge slat, variable droop leading edge, oscillatory jet, and Gurney flap-increased the blade maximum loading capability when these devices were used over the retreating side of the rotor disk. C1 US Army Res Dev & Engn Command, Ames Res Ctr, Aeroflightdynam Directorate, Moffett Field, CA USA. RP Yeo, HS (reprint author), US Army Res Dev & Engn Command, Ames Res Ctr, Aeroflightdynam Directorate, Moffett Field, CA USA. EM hsyeo@mail.arc.nasa.gov NR 31 TC 22 Z9 25 U1 0 U2 3 PU AMER HELICOPTER SOC INC PI ALEXANDRIA PA 217 N WASHINGTON ST, ALEXANDRIA, VA 22314 USA SN 0002-8711 J9 J AM HELICOPTER SOC JI J. Am. Helicopter Soc. PD APR PY 2008 VL 53 IS 2 BP 152 EP 163 PG 12 WC Engineering, Aerospace SC Engineering GA 288SS UT WOS:000255006700004 ER PT J AU Masarati, P Piatak, DJ Quaranta, G Singleton, JD Shen, JW AF Masarati, Pierangelo Piatak, David J. Quaranta, Giuseppe Singleton, Jeffrey D. Shen, Jinwei TI Soft-inplane tiltrotor aeromechanics investigation using two comprehensive multibody solvers SO JOURNAL OF THE AMERICAN HELICOPTER SOCIETY LA English DT Article ID SYSTEMS; ROTORCRAFT; STABILITY; MODEL AB This paper focuses on the development of multibody numerical models to predict the dynamic response, aeroelastic stability, and blade loading of a soft-inplane tiltrotor wind-tunnel model. Comprehensive rotorcraft-based multibody analyses enable modeling of the rotor system to a high level of detail such that complex mechanics and nonlinear effects associated with control system geometry, and joint deadband may be considered. The influence of these and other nonlinear effects on the aeromechanical behavior of the tiltrotor model is examined. To assess the reliability of the multibody approach to rotorcraft analysis, the results obtained using two different rotorcraft-based multibody solvers are analyzed and compared. A parametric study of some design parameters that may influence the aeromechanics of the soft-inplane rotor system is also included in this investigation. C1 [Masarati, Pierangelo; Quaranta, Giuseppe] Politecn Milan, Dipartimento Ingn Aerospaziale, I-20133 Milan, Italy. [Piatak, David J.] NASA, Langley Res Ctr, Aeroelast Branch, Hampton, VA 23665 USA. [Singleton, Jeffrey D.] Army Res Labs, Vehicle Technol Directorate, Hampton, VA USA. [Shen, Jinwei] Natl Inst Aerosp, Hampton, VA USA. RP Quaranta, G (reprint author), Politecn Milan, Dipartimento Ingn Aerospaziale, I-20133 Milan, Italy. EM quaranta@aero.polimi.it RI Masarati, Pierangelo/I-3898-2012; Quaranta, Giuseppe/F-7955-2012 OI Masarati, Pierangelo/0000-0002-9347-7654; Quaranta, Giuseppe/0000-0002-8873-7351 NR 33 TC 7 Z9 7 U1 0 U2 0 PU AMER HELICOPTER SOC INC PI ALEXANDRIA PA 217 N WASHINGTON ST, ALEXANDRIA, VA 22314 USA SN 0002-8711 J9 J AM HELICOPTER SOC JI J. Am. Helicopter Soc. PD APR PY 2008 VL 53 IS 2 BP 179 EP 192 DI 10.4050/JAHS.53.179 PG 14 WC Engineering, Aerospace SC Engineering GA 288SS UT WOS:000255006700006 ER PT J AU Yeo, HS Johnson, W AF Yeo, Hyeonsoo Johnson, Wayne TI Prediction of rotor structural loads with comprehensive analysis SO JOURNAL OF THE AMERICAN HELICOPTER SOCIETY LA English DT Article; Proceedings Paper CT 31st European Rotorcraft Forum CY SEP 13-15, 2005 CL Florence, ITALY ID HELICOPTER AB Blade flap and chord bending and torsion moments are investigated for five rotors operating at transition and high speed: H-34 in flight and wind tunnel, SA 330 (research Puma), SA 349/2, UH-60A full-scale, and BO-105 model (HART-I). The measured data from flight and wind tunnel tests are compared with calculations obtained using the comprehensive analysis CAMRAD II. The calculations were made using two free wake models: rolled-up and multiple-trailer with consolidation models. At transition speed, there is fair to good agreement for the flap and chord bending moments between the test data and analysis for the H-34, research Puma, and SA 349/2. Torsion moment correlation, in general, is fair to good for all the rotors investigated. Better flap bending and torsion moment correlation is obtained for the UH-60A and BO-105 rotors by using the multiple-trailer with consolidation wake model. In the high-speed condition, the analysis shows generally better correlation in magnitude than in phase for the flap bending and torsion moments. However, a significant underprediction of chord bending moment is observed for the research Puma and UH-60A. The poor correlation of the chord bending moment for the UH-60A appears to be caused by both the airloads model (at all radial locations) and the lag damper model (mostly at inboard locations). C1 [Yeo, Hyeonsoo] USA, Aeroflightdynam Directorate, Res Dev & Engn Command, Ames Res Ctr, Moffett Field, CA USA. [Johnson, Wayne] NASA, Ames Res Ctr, Aeromech Branch, Moffett Field, CA 94035 USA. RP Yeo, HS (reprint author), USA, Aeroflightdynam Directorate, Res Dev & Engn Command, Ames Res Ctr, Moffett Field, CA USA. EM hsyeo@mail.arc.nasa.gov NR 13 TC 21 Z9 22 U1 0 U2 3 PU AMER HELICOPTER SOC INC PI ALEXANDRIA PA 217 N WASHINGTON ST, ALEXANDRIA, VA 22314 USA SN 0002-8711 J9 J AM HELICOPTER SOC JI J. Am. Helicopter Soc. PD APR PY 2008 VL 53 IS 2 BP 193 EP 209 PG 17 WC Engineering, Aerospace SC Engineering GA 288SS UT WOS:000255006700007 ER PT J AU Luo, YL Xu, KM Morrison, H McFarquhar, G AF Luo, Yali Xu, Kuan-Man Morrison, Hugh McFarquhar, Greg TI Arctic mixed-phase clouds simulated by a cloud-resolving model: Comparison with ARM observations and sensitivity to microphysics parameterizations SO JOURNAL OF THE ATMOSPHERIC SCIENCES LA English DT Article ID RADIATIVE PROPERTIES; CLIMATE MODELS; ATMOSPHERIC RADIATION; STRATIFORM CLOUDS; CIRRUS CLOUDS; ACCURATE PARAMETERIZATION; AEROSOL ACTIVATION; ICE PARTICLES; WATER-VAPOR; CONVECTION AB Single-layer mixed-phase stratiform (MPS) Arctic clouds, which formed under conditions of large surface heat flux combined with general subsidence during a subperiod of the Atmospheric Radiation Measurement (ARM) Program's Mixed-Phase Arctic Cloud Experiment (MPACE), are simulated with a cloud-resolving model (CRM). The CRM is implemented with either an advanced two-moment [ Morrison et al. (MCK)] or a commonly used one-moment [Lin et al. (LFO)] bulk microphysics scheme and a state-of-the-art radiative transfer scheme. The MCK simulation, which uses the two-moment scheme and observed aerosol size distribution and ice nulei (IN) number concentration, reproduces the magnitudes and vertical structures of cloud liquid water content (LWC), total ice water content (IWC), and number concentration and effective radius of cloud droplets as suggested by the MPACE observations. The simulation underestimates ice crystal number concentrations by an order of magnitude and overestimates effective radius of ice crystals by a factor of 2-3. The LFO experiment, which uses the one-moment scheme, produces values of liquid water path (LWP) and ice plus snow water path (ISWP) that were about 30% and 4 times, respectively, those produced by MCK. The vertical profile of IWC exhibits a bimodal distribution in contrast to the constant distribution of IWC produced in MCK and observations. A sensitivity test that uses the same ice-water saturation adjustment scheme as in LFO produces cloud properties that are more similar to the LFO simulation than MCK. The mean value of the intercept parameter of snow size spectra (N-0s) from MCK is one order of magnitude smaller than that assumed in LFO. A sensitivity test that prescribes the larger LFO N-0s results in 20% less LWP and 5 times larger snow water path than that in MCK. When an exponential ice size distribution replaces the gamma size distribution in MCK, the ISWP decreases by 70% but the LWP increases by 7% versus that in the MCK. Increasing the IN number concentration from the observed value of 0.16 to 3.2 L-1 forces the MPS clouds to become glaciated and dissipate, but the simulated ice number concentration agrees initially with the observations better. Physical explanations for these quantitative differences are provided. It is further shown that the differences between the LFO and MCK results are larger than those due to the estimated uncertainties in the prescribed surface fluxes. Additional observations and simulations of a variety of cases are required to further narrow down uncertainties in the microphysics schemes. C1 [Luo, Yali] Natl Inst Aerosp, Hampton, VA USA. [Luo, Yali; Xu, Kuan-Man] NASA, Langley Res Ctr, Hampton, VA 23665 USA. [Morrison, Hugh] Natl Ctr Atmospher Res, Boulder, CO 80307 USA. [McFarquhar, Greg] Univ Illinois, Urbana, IL 61801 USA. RP Luo, YL (reprint author), Chinese Acad Meteorol Sci, State Key Lab Severe Weather, Beijing 100081, Peoples R China. EM yali@cams.cma.gov.cn RI Xu, Kuan-Man/B-7557-2013; OI Xu, Kuan-Man/0000-0001-7851-2629; McFarquhar, Greg/0000-0003-0950-0135 NR 63 TC 22 Z9 24 U1 0 U2 8 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 0022-4928 J9 J ATMOS SCI JI J. Atmos. Sci. PD APR PY 2008 VL 65 IS 4 BP 1285 EP 1303 DI 10.1175/2007JAS2467.1 PG 19 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 293VB UT WOS:000255362400009 ER PT J AU Sabato, JS AF Sabato, Jude S. TI CO2 condensation in baroclinic eddies on early Mars SO JOURNAL OF THE ATMOSPHERIC SCIENCES LA English DT Article ID CARBON-DIOXIDE CLOUDS; MARTIAN ATMOSPHERE; PLANETARY-ATMOSPHERES; RELATIVE-HUMIDITY; SIMPLIFIED MODEL; MASS SINK; CLIMATE; INSTABILITY; WAVE; MIDLATITUDE AB The efficacy of a cloud-radiative feedback on early Mars is reexamined in the context of the theory of baroclinic waves in midlatitudes. The feedback has been proposed to explain fluvial features on the surface of Mars. The radiative-convective models used to calculate the magnitude of the feedback require knowledge of the cloud depth, thickness, and areal coverage. Using a quasigeostrophic model and primitive equation simulations, it seems that less than 50% areal cloud cover is likely for early Mars, at least in midlatitudes. In accordance with previous studies for Earth, when condensational heating is included, the updraft region is narrower than in dry eddies. This results in reduced cloud cover and the feedback being weaker than previously thought. The simulations also show that condensation in eddies may have been important on a thick but cold early Mars but that its effects are much weaker for warmer climates. C1 [Sabato, Jude S.] CALTECH, Jet Prop Lab, Pasadena, CA USA. RP Sabato, JS (reprint author), SW Res Inst, Dept Space Studies, 1050 Walnut St,Suite 300, Boulder, CO 80302 USA. EM jssabato@boulder.swri.edu NR 47 TC 3 Z9 3 U1 0 U2 0 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 0022-4928 J9 J ATMOS SCI JI J. Atmos. Sci. PD APR PY 2008 VL 65 IS 4 BP 1378 EP 1395 DI 10.1175/2007JAS2504.1 PG 18 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 293VB UT WOS:000255362400014 ER PT J AU Grudinin, IS Maleki, L AF Grudinin, Ivan S. Maleki, Lute TI Efficient Raman laser based on a CaF2 resonator SO JOURNAL OF THE OPTICAL SOCIETY OF AMERICA B-OPTICAL PHYSICS LA English DT Article ID WHISPERING-GALLERY MODES; OPTICAL MICROCAVITIES; SCATTERING; CAVITY AB We report on an ultralow-threshold Raman laser based on a CaF2 whispering-gallery-mode resonator. The laser is demonstrated to have a conversion efficiency above 60%. The observed low lasing threshold is made possible by the ultrahigh optical quality factor of the cavity, which is on the order of Q = 10(10). The laser is fiber-compatible and is fabricated with a very simple technique. We also demonstrate a single-mode operation of the laser in a multimode cavity as well as a multimode operation of the laser in a single-mode cavity. (C) 2008 Optical Society of America. C1 [Grudinin, Ivan S.; Maleki, Lute] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Maleki, Lute] OEwaves, Pasadena, CA 91106 USA. RP Grudinin, IS (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM grudinin@caltech.edu NR 18 TC 20 Z9 20 U1 1 U2 7 PU OPTICAL SOC AMER PI WASHINGTON PA 2010 MASSACHUSETTS AVE NW, WASHINGTON, DC 20036 USA SN 0740-3224 J9 J OPT SOC AM B JI J. Opt. Soc. Am. B-Opt. Phys. PD APR PY 2008 VL 25 IS 4 BP 594 EP 598 DI 10.1364/JOSAB.25.000594 PG 5 WC Optics SC Optics GA 294MS UT WOS:000255410700014 ER PT J AU Bynum, MD Hollis, BR Hassan, HA Xiao, X AF Bynum, Michael D. Hollis, Brian R. Hassan, H. A. Xiao, X. TI Turbulent aeroheating on the mars science laboratory entry vehicle SO JOURNAL OF THERMOPHYSICS AND HEAT TRANSFER LA English DT Article; Proceedings Paper CT AIAA 39th Thermophysics Conference CY JUN 25-28, 2007 CL Miami, FL SP AIAA C1 [Bynum, Michael D.; Hassan, H. A.; Xiao, X.] N Carolina State Univ, Raleigh, NC 27695 USA. [Hollis, Brian R.] NASA, Langley Res Ctr, Aerothermodynam Branch, Hampton, VA 23681 USA. RP Bynum, MD (reprint author), N Carolina State Univ, Raleigh, NC 27695 USA. NR 7 TC 0 Z9 0 U1 0 U2 0 PU AMER INST AERONAUT ASTRONAUT PI RESTON PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA SN 0887-8722 J9 J THERMOPHYS HEAT TR JI J. Thermophys. Heat Transf. PD APR-JUN PY 2008 VL 22 IS 2 BP 306 EP 309 DI 10.2514/1.33281 PG 4 WC Thermodynamics; Engineering, Mechanical SC Thermodynamics; Engineering GA 288DV UT WOS:000254967300022 ER PT J AU Hamilton, D Smart, K Melton, S Polk, JD Johnson-Throop, K AF Hamilton, Douglas Smart, Kieran Melton, Shannon Polk, James D. Johnson-Throop, Kathy TI Autonomous medical care for exploration class space missions SO JOURNAL OF TRAUMA-INJURY INFECTION AND CRITICAL CARE LA English DT Article ID BREAST-CANCER; PNEUMOTHORAX; STRATEGIES; TRAUMA; DEATH AB The US-based health care system of the International Space Station contains several subsystems, the Health Maintenance System, Environmental Health System and the Countermeasure System. These systems are designed to provide primary, secondary and tertiary medical prevention strategies. The medical system deployed in low Earth orbit for the International Space Station is designed to support a "stabilize and transport" concept of operations. In this paradigm, an ill or injured crewmember would be rapidly evacuated to a definitive medical care facility (DMCF) on Earth, rather than being treated for a protracted period on orbit. The medical requirements of the short (7 day) and long duration (up to 6 months) exploration class missions to the moon are similar to low Earth orbit class missions but also include an additional 4 to 5 days needed to transport an ill or injured crewmember to a DMCF on Earth. Mars exploration class missions are quite different in that they will significantly delay or prevent the return of an ill or injured crewmember to a DMCF. In addition the limited mass, power and volume afforded to medical care will prevent the mission designers from manifesting the entire capability of terrestrial care. National Aeronautics and Space Administration has identified five levels of care as part of its approach to medical support of future missions including the Constellation program. To implement an effective medical risk mitigation strategy for exploration class missions, modifications to the current suite of space medical systems may be needed, including new crew medical officer training methods, treatment guidelines, diagnostic and therapeutic resources, and improved medical informatics. C1 [Hamilton, Douglas; Smart, Kieran; Melton, Shannon] Wyle Life Sci, Houston, TX 77058 USA. [Polk, James D.; Johnson-Throop, Kathy] NASA, Med Operat & Healthcare Syst, Washington, DC 20546 USA. RP Hamilton, D (reprint author), Wyle Life Sci, 1290 Hercules Dr,Suite 120, Houston, TX 77058 USA. EM dhamilton@wylehou.com NR 19 TC 4 Z9 5 U1 1 U2 3 PU LIPPINCOTT WILLIAMS & WILKINS PI PHILADELPHIA PA 530 WALNUT ST, PHILADELPHIA, PA 19106-3621 USA SN 0022-5282 J9 J TRAUMA JI J. Trauma-Injury Infect. Crit. Care PD APR PY 2008 VL 64 IS 4 SU S BP S354 EP S363 DI 10.1097/TA.0b013e31816c005d PG 10 WC Critical Care Medicine; Surgery SC General & Internal Medicine; Surgery GA 288WT UT WOS:000255017400008 PM 18385587 ER PT J AU Kerrebrock, JL Epstein, AH Merchant, AA Guenette, GR Parker, D Onnee, JF Neumayer, F Adamczyk, JJ Shabbir, A AF Kerrebrock, Jack L. Epstein, Alan H. Merchant, Ali A. Guenette, Gerald R. Parker, David Onnee, Jean-Francois Neumayer, Fritz Adamczyk, John J. Shabbir, Aamir TI Design and test of an aspirated counter-rotating fan SO JOURNAL OF TURBOMACHINERY-TRANSACTIONS OF THE ASME LA English DT Article ID COMPRESSOR AB The design and test of a two-stage, vaneless, aspirated counter-rotating fan is presented in this paper. The fan nominal design objectives were a pressure ratio of 3:1 and adiabatic efficiency of 87%. A pressure ratio of 2.9 at 89% efficiency was measured at the design speed. The configuration consists of a counter-swirl-producing inlet guide vane, followed by a high tip speed (1450 ft/s) nonaspirated rotor and a counter-rotating low speed (1150 ft/s) aspirated rotor. The lower tip speed and lower solidity of the second rotor result in a blade loading above conventional limits, but enable a balance between the shock loss and viscous boundary layer loss; the latter of which can be controlled by aspiration. The aspiration slot on the second rotor suction surface extends from the hub up to 80% span. The bleed flow is discharged inward through the blade hub. This fan was tested in a short duration blowdown facility. Particular attention was given to the design of the instrumentation to measure efficiency to 0.5% accuracy. High response static pressure measurements were taken between the rotors and downstream of the fan to determine the stall behavior. Pressure ratio, mass flow, and efficiency on speed lines from 90% to 102% of the design speed are presented and discussed along with comparison to computational fluid dynamics predictions and design intent. The results presented here complement those presented earlier for two aspirated fan stages with tip shrouds, extending the validated design space for aspirated compressors to include designs with conventional unshrouded rotors and with inward removal of the aspirated flow. C1 [Kerrebrock, Jack L.; Epstein, Alan H.; Merchant, Ali A.; Guenette, Gerald R.; Parker, David; Onnee, Jean-Francois; Neumayer, Fritz] MIT, Gas Turbine Lab, Cambridge, MA 02139 USA. [Adamczyk, John J.] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. [Shabbir, Aamir] Univ Toledo, Toledo, OH 43606 USA. RP Kerrebrock, JL (reprint author), MIT, Gas Turbine Lab, 77 Massachusetts Ave, Cambridge, MA 02139 USA. NR 20 TC 6 Z9 11 U1 1 U2 11 PU ASME-AMER SOC MECHANICAL ENG PI NEW YORK PA THREE PARK AVE, NEW YORK, NY 10016-5990 USA SN 0889-504X J9 J TURBOMACH JI J. Turbomach.-Trans. ASME PD APR PY 2008 VL 130 IS 2 AR 021004 DI 10.1115/1.2776951 PG 8 WC Engineering, Mechanical SC Engineering GA 279UP UT WOS:000254380800004 ER PT J AU Templeton, TC AF Templeton, Thomas Clay TI Placing the library: An argument for the phenomenological and constructivist approach to the human geography of the library SO LIBRARY QUARTERLY LA English DT Article ID INFORMATION AB Place reminds us to tailor our professional work to the shifting concerns, and indeed the shifting criteria, of our shifting constituencies, rather than to a placeless professional vision of what librarianship, society, and literacy should be. Every place maker must make do, make sense, and make place in an environment that is technologically heterogeneous and in which the potential for novelty as well as recurrence is a persistent feature. The siege flag of place has been raised, not only in librarianship but in many sectors, in defense of the human and the parochial, of tradition and local turf. Taking a phenomenological cue, here we attempt to prune and redirect this problematic term. We arrive at what we consider reasonable criteria of success for ourselves: to what extent is our "library," in whatever professional sense we assign that word, vitally connected to the discursive practices of the places from which it draws its mandate? We contend that vitalizing a library in this respect requires us to step outside the sphere of our habitual familiarity and to explore other places. How we go about doing this is a matter of methodology. If a prior conception of place interferes with the absorption of ethnomethods, it should be held in suspension, bracketed at least until the practitioner can grasp the place that already exists. C1 NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Templeton, TC (reprint author), NASA, Goddard Space Flight Ctr, Code 305-0,8800 Greenbelt Rd, Greenbelt, MD 20771 USA. NR 53 TC 6 Z9 6 U1 1 U2 3 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0024-2519 J9 LIBR QUART JI Libr. Q. PD APR PY 2008 VL 78 IS 2 BP 195 EP 209 DI 10.1086/528889 PG 15 WC Information Science & Library Science SC Information Science & Library Science GA 271FM UT WOS:000253774300003 ER PT J AU Cintala, MJ Horz, F AF Cintala, Mark J. Hoerz, Friedrich TI Experimental impacts into chondritic targets, part I: Disruption of an L6 chondrite by multiple impacts SO METEORITICS & PLANETARY SCIENCE LA English DT Article ID HIGH-VELOCITY IMPACT; COLLISIONAL DISRUPTION; ASTEROIDS; METEORITES; DENSITY; POROSITY; FRAGMENTATION; DESTRUCTION; SIMULATION; REGOLITHS AB A fragment of an L6 chondrite (Allan Hills [ALH] 85017,13) with an initial mass (M-0) of 464.1 g was the target in a series of experimental impacts in which the largest remaining fragment (M-R) after each shot was impacted by a 3.18 mm ceramic sphere at a nominal speed of 2 km s(-1). This continued until the mass of the largest remaining piece was less than half the mass of the target presented to that shot (M-S). Two chunks of Bushveldt gabbro with similar initial masses were also impacted under the same conditions until M-R was less than half M-0. The two gabbro targets required a total of 1.51 x 10(7) and 1.75 x 10(7) erg g(-1) to attain 0.27 and 0.33 M-R/M-0, respectively; the chondrite, however, was considerably tougher, reaching 0.40 and 0.21 M-R/M-0 only after receiving 2.37 x 10(7) and 3.10 x 10(7) erg g(-1), respectively. The combined ejecta and spallation products from the gabbro impacts were coarser than those from the chondrite and in sufficient quantities that the new surface areas exceeded those from the meteorite until the fifth shot in the chondrite series, which was the number of impacts required to disrupt each gabbro target (i.e., M-R/M-0 <= 0.5). Unlike the behavior shown in previous regolith-evolution series, neither gabbro target produced an enhancement in the size fraction reflecting the mean size of the crystals composing the rock (about 3 mm), an effect possibly related to the width of the shock pulse. The original chondrite was so fine-grained and fractured, and the variance in its grain-size distribution so large, that effects related to grain size were relegated to the <63 mu m fraction. Impacts into ALH 85017 produced abundant, fine-grained debris, but otherwise the slopes of its size distributions were comparable to those from other experiments involving natural and fabricated terrestrial targets. The characteristic slopes of the chondrite's size distributions, however, were notably more constant over the entire nine-impact series than those from any of-the terrestrial targets, a testament to the control over comminution apparently exerted by pre-existing fractures and other, microscopic damage in the meteorite. The enhancement in the finer fraction of debris from ALH 85017 indicates that ordinary chondrites in solar orbit would be very efficient contributors to the cosmic-dust complex. At the same time, the greater resistance to disruption displayed by ordinary chondrites relative to that exhibited by igneous rocks indicates that a selection effect could be operative between the annealed, ordinary-chondritic breccias and relatively weaker, differentiated meteorites. Preferential survival from their time in the regoliths of their parent bodies through their transit to Earth and passage through the atmosphere suggests that meteorite collections could be biased in favor of the ordinary chondrites. C1 [Cintala, Mark J.; Hoerz, Friedrich] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. RP Cintala, MJ (reprint author), NASA, Lyndon B Johnson Space Ctr, Code KR, Houston, TX 77058 USA. EM mark.j.cintala@nasa.gov NR 56 TC 8 Z9 8 U1 2 U2 7 PU METEORITICAL SOC PI FAYETTEVILLE PA DEPT CHEMISTRY/BIOCHEMISTRY, UNIV ARKANSAS, FAYETTEVILLE, AR 72701 USA SN 1086-9379 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD APR PY 2008 VL 43 IS 4 BP 771 EP 803 PG 33 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 346BX UT WOS:000259044500010 ER PT J AU Mackenzie, AI Baginski, ME Rao, SM AF Mackenzie, Anne I. Baginski, Michael E. Rao, Sadasiva M. TI New basis functions for the electromagnetic solution of arbitrarily-shaped, three dimensional conducting bodies using method of moments SO MICROWAVE AND OPTICAL TECHNOLOGY LETTERS LA English DT Article DE method of moments; electromagnetics; scattering ID SCATTERING; FIELD AB In this work, we present a new set of basis functions, defined over a pair of planar triangular patches, for the solution of electromagnetic scattering and radiation problems associated with arbitrarily-shaped surfaces using the method of moments solution procedure. The basis functions are constant over the function subdomain and resemble pulse functions for one and two dimensional problems. Further, another set of basis functions, point-wise orthogonal to the first set, is also defined over the same function space. The primary objective of developing these basis functions is to utilize them for the electromagnetic solution involving conducting, dielectric, and composite bodies. However, in the present work, only the conducting body solution is presented and compared with other data. (C) 2008 Wiley Periodicals, Inc. C1 [Baginski, Michael E.; Rao, Sadasiva M.] Auburn Univ, Dept E & CE, Auburn, AL 36849 USA. [Mackenzie, Anne I.] NASA, Langley Res Ctr, Hampton, VA 23681 USA. RP Rao, SM (reprint author), Auburn Univ, Dept E & CE, Auburn, AL 36849 USA. EM rao@eng.auburn.edu NR 6 TC 2 Z9 2 U1 0 U2 1 PU JOHN WILEY & SONS INC PI HOBOKEN PA 111 RIVER ST, HOBOKEN, NJ 07030 USA SN 0895-2477 J9 MICROW OPT TECHN LET JI Microw. Opt. Technol. Lett. PD APR PY 2008 VL 50 IS 4 BP 1121 EP 1124 DI 10.1002/mop.23295 PG 4 WC Engineering, Electrical & Electronic; Optics SC Engineering; Optics GA 275EW UT WOS:000254055700080 ER PT J AU Yang, SC Kalnay, E Cai, M Rienecker, MM AF Yang, Shu-Chih Kalnay, Eugenia Cai, Ming Rienecker, Michele M. TI Bred vectors and tropical Pacific forecast errors in the NASA coupled general circulation model SO MONTHLY WEATHER REVIEW LA English DT Article ID ENSEMBLE KALMAN FILTER; OCEAN-ATMOSPHERE MODEL; 4-DIMENSIONAL VARIATIONAL ASSIMILATION; NINO SOUTHERN-OSCILLATION; MADDEN-JULIAN OSCILLATION; 1997-98 EL-NINO; SINGULAR VECTORS; INITIAL CONDITIONS; EQUATORIAL WAVES; ENSO AB The breeding method has been implemented in the NASA Global Modeling and Assimilation Office coupled general circulation model (CGCM) in its operational configuration in which ocean data assimilation is used to initialize the coupled forecasts. Bred vectors (BVs), designed to capture the dominant growing errors in the atmosphere-ocean coupled system, are applied as initial ensemble perturbations. The potential improvement for ensemble prediction is investigated by comparing BVs with the oceanic growing errors, estimated by the one-month forecast error from the nonperturbed forecast. Results show that one-month forecast errors and BVs from the NASA CGCM share very similar features: BVs are clearly related to forecast errors in both SST and equatorial subsurface temperature-in particular, when the BV growth rate is large. Both the forecast errors and the BVs in the subsurface are dominated by large-scale structures near the thermocline. Results suggest that the forecast errors are dominated by dynamically evolving structures related to the variations of the background anomalous state, and that their shapes can be captured by BVs, especially during the strong 1997/98 El Nino. Hindcast experiments starting from January 1997 with one pair of BVs achieve a significant improvement relative to the control (unperturbed) hindcast by capturing many important features of this event, including the westerly wind burst in early 1997. C1 [Yang, Shu-Chih; Kalnay, Eugenia] Univ Maryland, Dept Atmospher & Ocean Sci, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20742 USA. [Yang, Shu-Chih; Rienecker, Michele M.] NASA, Goddard Space Flight Ctr, Global Modeling & Assimilat Off, Greenbelt, MD 20771 USA. [Cai, Ming] Florida State Univ, Dept Meteorol, Tallahassee, FL 32306 USA. RP Yang, SC (reprint author), Univ Maryland, Dept Atmospher & Ocean Sci, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20742 USA. EM scyang@atmos.umd.edu RI Kalnay, Eugenia/F-4393-2010; OI Kalnay, Eugenia/0000-0002-9984-9906 NR 66 TC 13 Z9 13 U1 0 U2 2 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 APR PY 2008 VL 136 IS 4 BP 1305 EP 1326 DI 10.1175/2007MWR2118.1 PG 22 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 293RK UT WOS:000255352200004 ER PT J AU Carrier, MJ Zou, X Lapenta, WM AF Carrier, Matthew J. Zou, Xiaolei Lapenta, William M. TI Comparing the vertical structures of weighting functions and adjoint sensitivity of radiance and verifying mesoscale forecasts using AIRS radiance observations SO MONTHLY WEATHER REVIEW LA English DT Article ID MODEL; ASSIMILATION; SYSTEM AB An adjoint sensitivity analysis is conducted using the adjoint of the hyperspectral radiative transfer model (RTM) that simulates the radiance spectrum from the Advanced Infrared Sounder (AIRS). It is shown, both theoretically and numerically, that the height of the maximum sensitivity of radiance in a channel could be higher or lower than the height of the maximum weighting function of that channel. It is shown that the discrepancy between the two heights is determined by the vertical structures of the atmospheric thermodynamic state. The sensitivity finds the level at which changes in temperature and/or moisture will have the largest influence on the simulated brightness temperature (BT), and the maximum weighting function (WF) height indicates the level where the model atmosphere contributes most significantly to the emission at the top of the atmosphere. Based on the above findings, an adjoint method for forecast verification using AIRS radiances is presented. In this method, model forecasts are first mapped into radiance space by an RTM so that they can be compared directly with the observed radiance values. The adjoint sensitivity analysis results are then used to connect the deviations of the model forecasts from observed radiances to the changes of temperature and moisture variables in model space. This adjoint sensitivity based model verification provides useful information on forecast model performances based on indirect observations from satellites. C1 [Carrier, Matthew J.; Zou, Xiaolei] Florida State Univ, Dept Meteorol, Tallahassee, FL 32306 USA. [Lapenta, William M.] NASA, George C Marshall Space Flight Ctr, Global Hydrol & Climate Ctr, Huntsville, AL 35812 USA. RP Carrier, MJ (reprint author), Florida State Univ, Dept Meteorol, 404 Love Bldg, Tallahassee, FL 32306 USA. EM mcarrier@met.fsu.edu NR 17 TC 1 Z9 1 U1 0 U2 3 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 APR PY 2008 VL 136 IS 4 BP 1327 EP 1348 DI 10.1175/2007MWR2057.1 PG 22 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 293RK UT WOS:000255352200005 ER PT J AU LaCasse, KM Splitt, ME Lazarus, SM Lapenta, WM AF LaCasse, Katherine M. Splitt, Michael E. Lazarus, Steven M. Lapenta, William M. TI The impact of high-resolution sea surface temperatures on the simulated nocturnal Florida marine boundary layer SO MONTHLY WEATHER REVIEW LA English DT Article ID EASTERN EQUATORIAL PACIFIC; TROPICAL INSTABILITY WAVES; WIND STRESS; REAL-TIME; PART I; NUMERICAL-SIMULATION; MESOSCALE ANALYSIS; AGULHAS CURRENT; RETURN CURRENT; SST VARIATIONS AB High- and low-resolution sea surface temperature (SST) analysis products are used to initialize the Weather Research and Forecasting (WRF) Model for May 2004 for short-term forecasts over Florida and surrounding waters. Initial and boundary conditions for the simulations were provided by a combination of observations, large-scale model output, and analysis products. The impact of using a l-km Moderate Resolution Imaging Spectroradiometer (MODIS) SST composite on subsequent evolution of the marine atmospheric boundary layer (MABL) is assessed through simulation comparisons and limited validation. Model results are presented for individual simulations, as well as for aggregates of easterly- and westerly-dominated low-level flows. The simulation comparisons show that the use of MODIS SST composites results in enhanced convergence zones, earlier and more intense horizontal convective rolls, and an increase in precipitation as well as a change in precipitation location. Validation of 10-m winds with buoys shows a slight improvement in wind speed. The most significant results of this study are that 1) vertical wind stress divergence and pressure gradient accelerations across the Florida Current region vary in importance as a function of flow direction and stability and 2) the warmer Florida Current in the MODIS product transports heat vertically and downwind of this heat source, modifying the thermal structure and the MABL wind field primarily through pressure gradient adjustments. C1 [LaCasse, Katherine M.] Univ Alabama, Huntsville, AL 35805 USA. [Splitt, Michael E.; Lazarus, Steven M.] Florida Inst Technol, Melbourne, FL 32901 USA. [Lapenta, William M.] NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA. RP LaCasse, KM (reprint author), Univ Alabama, 320 Sparkman Dr, Huntsville, AL 35805 USA. EM kate.lacasse@nasa.gov OI Splitt, Michael/0000-0002-7690-5100; Lazarus, Steven/0000-0002-5918-1059 NR 48 TC 17 Z9 17 U1 0 U2 2 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 APR PY 2008 VL 136 IS 4 BP 1349 EP 1372 DI 10.1175/2007MWR2167.1 PG 24 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 293RK UT WOS:000255352200006 ER PT J AU Schmidt, G AF Schmidt, Gavin TI To blog or not to blog? SO NATURE GEOSCIENCE LA English DT Editorial Material C1 Columbia Univ, NASA, Goddard Inst Space Studies, New York, NY 10025 USA. RP Schmidt, G (reprint author), Columbia Univ, NASA, Goddard Inst Space Studies, 2880 Broadway, New York, NY 10025 USA. EM Gavin.A.schmidt@nasa.gov RI Schmidt, Gavin/D-4427-2012 OI Schmidt, Gavin/0000-0002-2258-0486 NR 0 TC 9 Z9 9 U1 0 U2 4 PU NATURE PUBLISHING GROUP PI NEW YORK PA 75 VARICK STREET, 9TH FLOOR, NEW YORK, NY 10013-1917 USA SN 1752-0894 J9 NAT GEOSCI JI Nat. Geosci. PD APR PY 2008 VL 1 IS 4 BP 208 EP 208 DI 10.1038/ngeo170 PG 1 WC Geosciences, Multidisciplinary SC Geology GA 309BA UT WOS:000256433500005 ER PT J AU Connolly, PJ Jezorek, IG Martens, KD Prentice, EF AF Connolly, Patrick J. Jezorek, Ian G. Martens, Kyle D. Prentice, Earl F. TI Measuring the performance of two stationary interrogation systems for detecting downstream and upstream movement of PIT-tagged salmonids SO NORTH AMERICAN JOURNAL OF FISHERIES MANAGEMENT LA English DT Article ID JUVENILE ATLANTIC SALMON; INTEGRATED TRANSPONDER TAGS; CHINOOK SALMON; HABITAT USE; COLUMBIA RIVERS; SMALL STREAMS; FISH; SURVIVAL; BEHAVIOR; SNAKE AB We tested the performance of two stationary interrogation systems designed for detecting the movement of fish with passive integrated transponder (PIT) tags. These systems allowed us to determine the direction of fish movement with high detection efficiency and high precision in a dynamic stream environment. We describe an indirect method for deriving an estimate for detection efficiency and the associated variance that does not rely on a known number of fish passing the system. By using six antennas arranged in a longitudinal series of three arrays, we attained detection efficiencies for downstream- and upstream-moving fish exceeding 96% during high-flow periods and approached 100% during low-flow periods for the two interrogation systems we tested. Because these systems did not rely on structural components, such as bridges or culverts, they were readily adaptable to remote, natural stream sites. Because of built-in redundancy, these systems were able to perform even with a loss of one or more antennas owing to dislodgement or electrical failure. However, the reduction in redundancy resulted in decreased efficiency and precision and the potential loss of ability to determine the direction of fish movement. What we learned about these systems should be applicable to a wide variety of other antenna configurations and to other types of PIT tags and transceivers. C1 [Connolly, Patrick J.; Jezorek, Ian G.; Martens, Kyle D.] Western Fisheries Res Ctr, Columbia River Res Lab, US Geol Survey, Cook, WA 98605 USA. [Prentice, Earl F.] Manchester Res Field Stn, Natl Marine Fisheries Serv, Manchester, WA 98353 USA. RP Connolly, PJ (reprint author), Western Fisheries Res Ctr, Columbia River Res Lab, US Geol Survey, 5501A Cook-Underwood Rd, Cook, WA 98605 USA. EM pconnolly@usgs.gov NR 34 TC 30 Z9 30 U1 4 U2 18 PU AMER FISHERIES SOC PI BETHESDA PA 5410 GROSVENOR LANE SUITE 110, BETHESDA, MD 20814-2199 USA SN 0275-5947 J9 N AM J FISH MANAGE JI North Am. J. Fish Manage. PD APR PY 2008 VL 28 IS 2 BP 402 EP 417 DI 10.1577/M07-008.1 PG 16 WC Fisheries SC Fisheries GA 293BR UT WOS:000255310300007 ER PT J AU Moiseev, AA AF Moiseev, A. A. TI Gamnia-ray large area space telescope: Mission overview SO NUCLEAR INSTRUMENTS & METHODS IN PHYSICS RESEARCH SECTION A-ACCELERATORS SPECTROMETERS DETECTORS AND ASSOCIATED EQUIPMENT LA English DT Article; Proceedings Paper CT 1st Roma International Conference on Astroparticle Physics CY JUN 20-22, 2007 CL Rome, ITALY DE gamma-ray telescope; gamma rays; gamma-ray burst; AGN; pulsar; SNR ID GLAST; TESTS AB The new Gamma-ray Large Area Space Telescope (GLAST) is scheduled for launch in the middle of 2008. It contains the high energy gamma-ray telescope Large Area Telescope (LAT) which covers the energy range from 20 MeV to > 300 GeV and the GLAST Burst Monitor (GMB), covering 8 keV-30 MeV energy range. The GLAST science objectives include understanding the mechanism of charged particle acceleration in active galactic nuclei, pulsars and supernova remnants, determining the nature of the still-unidentified EGRET sources, detailed study of gamma-ray diffuse emission, high-energy emission from gamma-ray bursts and transient sources, and probing dark matter. A brief overview of the mission is given. (c) 2008 Elsevier B.V. All rights reserved. C1 [Moiseev, A. A.] NASA, Goddard Space Flight Ctr, CRESST, Greenbelt, MD 20771 USA. [Moiseev, A. A.] NASA, Goddard Space Flight Ctr, Astroparticle Phys Lab, Greenbelt, MD 20771 USA. RP Moiseev, AA (reprint author), NASA, Goddard Space Flight Ctr, CRESST, Greenbelt, MD 20771 USA. EM alexander.a.moiseev@nasa.gov NR 10 TC 8 Z9 8 U1 0 U2 1 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0168-9002 J9 NUCL INSTRUM METH A JI Nucl. Instrum. Methods Phys. Res. Sect. A-Accel. Spectrom. Dect. Assoc. Equip. PD APR 1 PY 2008 VL 588 IS 1-2 BP 41 EP 47 DI 10.1016/j.nima.2008.01.005 PG 7 WC Instruments & Instrumentation; Nuclear Science & Technology; Physics, Nuclear; Physics, Particles & Fields SC Instruments & Instrumentation; Nuclear Science & Technology; Physics GA 295RF UT WOS:000255490900010 ER PT J AU Emfietzoglou, D Abril, I Garcia-Molina, R Petsalakis, ID Nikjoo, H Kyriakou, I Pathak, A AF Emfietzoglou, D. Abril, I. Garcia-Molina, R. Petsalakis, I. D. Nikjoo, H. Kyriakou, I. Pathak, A. TI Semi-empirical dielectric descriptions of the Bethe surface of the valence bands of condensed water SO NUCLEAR INSTRUMENTS & METHODS IN PHYSICS RESEARCH SECTION B-BEAM INTERACTIONS WITH MATERIALS AND ATOMS LA English DT Article; Proceedings Paper CT 18th International Conference on Ion Beam Analysis CY SEP 23-28, 2007 CL Univ Hyderabad, Sch Phys, Hyderabad, INDIA SP Inter Univ Accelerator Ctr, Inst Phys HO Univ Hyderabad, Sch Phys DE inelastic scattering; Bethe surface; Bethe ridge; dielectric function; energy loss function; water; ice ID MONTE-CARLO-SIMULATION; LOW-ENERGY ELECTRONS; X-RAY-SCATTERING; INELASTIC CROSS-SECTIONS; MEAN FREE PATHS; LIQUID WATER; STOPPING POWERS; OPTICAL-DATA; SECONDARY-ELECTRON; CHARGED-PARTICLES AB The Bethe surface of a material is an essential element in the study of inelastic scattering at low impact energies where the optical approximation fails. In this work we examine various semi-empirical models for the dielectric response function of condensed water towards an improved description of the energy-loss function over the whole energy-momentum plane (i.e. Bethe surface). The experimental "optical" data (i.e. at zero momentum transfer) for the valence bands of liquid and solid water are analytically represented by a sum-rule constrained linear combination of Drude-type functions. The dependence on momentum transfer is introduced through various widespread "extension" schemes which are compared against the available Compton scattering data. It is shown that the widely used Lindhard function along with its "single-pole" (or "delta-oscillator") approximation used in the Penn and Ashley models, as well as the Ritchie and Howie extended-Drude scheme with a simple quadratic dispersion, predict a sharp Bethe ridge which compares poorly with the experimental profile. In contrast, the Mermin dielectric function provides a more realistic account of the observed broadening with momentum transfer. An improved fully-extended-Drude model is presented which incorporates the momentum broadening and line-shift of the Bethe ridge and distinguishes between the different dispersion of the discrete and continuum spectra of water. (c) 2007 Elsevier B.V. All rights reserved. C1 [Pathak, A.] Univ Hyderabad, Sch Phys, Hyderabad 500046, Andhra Pradesh, India. [Emfietzoglou, D.; Kyriakou, I.] Univ Ioannina, Sch Med, Med Phys Lab, GR-45110 Ioannina, Greece. [Abril, I.] Univ Alicante, Dept Fis Aplicada, E-03080 Alicante, Spain. [Garcia-Molina, R.] Univ Murcia, Dept Fis CIOyN, E-30080 Murcia, Spain. [Petsalakis, I. D.] Natl Hellen Res Fdn, Inst Theoret & Phys Chem, GR-11635 Athens, Greece. [Nikjoo, H.] USRA, NASA Johnson Space Ctr, Ctr Adv Space Studies, Houston, TX 77058 USA. RP Pathak, A (reprint author), Univ Hyderabad, Sch Phys, Hyderabad 500046, Andhra Pradesh, India. EM appsp@uohyd.ernet.in RI Emfietzoglou, Dimitris/G-7168-2012; nhrf, tpci/M-8699-2013; Abril, Isabel/L-6938-2014; Garcia-Molina, Rafael/L-5679-2014 OI Abril, Isabel/0000-0001-9366-3484; Garcia-Molina, Rafael/0000-0001-8755-8709 NR 52 TC 21 Z9 21 U1 1 U2 20 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0168-583X J9 NUCL INSTRUM METH B JI Nucl. Instrum. Methods Phys. Res. Sect. B-Beam Interact. Mater. Atoms PD APR PY 2008 VL 266 IS 8 BP 1154 EP 1161 DI 10.1016/j.nimb.2007.11.057 PG 8 WC Instruments & Instrumentation; Nuclear Science & Technology; Physics, Atomic, Molecular & Chemical; Physics, Nuclear SC Instruments & Instrumentation; Nuclear Science & Technology; Physics GA 312NH UT WOS:000256677600003 ER PT J AU Bousis, C Emfietzoglou, D Hadjidoukas, P Nikjoo, H Pathak, A AF Bousis, C. Emfietzoglou, D. Hadjidoukas, P. Nikjoo, H. Pathak, A. TI Electron ionization cross-section calculations for liquid water at high impact energies SO NUCLEAR INSTRUMENTS & METHODS IN PHYSICS RESEARCH SECTION B-BEAM INTERACTIONS WITH MATERIALS AND ATOMS LA English DT Article; Proceedings Paper CT 18th International Conference on Ion Beam Analysis CY SEP 23-28, 2007 CL Univ Hyderabad, Sch Phys, Hyderabad, INDIA SP Inter Univ Accelerator Ctr, Inst Phys HO Univ Hyderabad, Sch Phys DE electrons; ionization; cross-sections; water ID INELASTIC-SCATTERING; SECONDARY ELECTRONS; CHARGED PARTICLES; CONDENSED MATTER; TRACK-STRUCTURE; MOLECULES; MODEL; COLLISIONS; ATOMS; H2O AB Cross-sections for the ionization of liquid water is perhaps the most essential set of data needed for modeling electron transport in biological matter. The complexity of ab initio calculations for any multi-electron target has led to largely heuristic semi-empirical models which take advantage elements of the Bethe, dielectric and binary collision theories. In this work we present various theoretical models for calculating total ionization cross-sections (TICSs) for liquid water over the 10 keV-1 MeV electron energy range. In particular, we extend our recent dielectric model calculations for liquid water to relativistic energies using both the appropriate kinematic corrections and the transverse part. Comparisons are made with widely used atomic and molecular TICS models such as those of Khare and co-workers, Kim-Rudd, Deutsch-Mark, Vriens and Gryzinski. The required dipole oscillator strength was provided by our recent optical-data model which is based on the latest experimental data for liquid water. The TICSs computed by the above models differ by up to 40% from the dielectric results. The best agreement (to within similar to 10%) was obtained by Khare's original model and an approximate form of Gryzinski's model. In contrast, the binary-encounter-dipole (BED) models of both Kim-Rudd and Khare and co-workers resulted in similar to 10-20% higher TICS values, while discrepancies increased to similar to 30-40% when their simpler binary-encounter-Bethe (BEB) versions were used. Finally, we discuss to what extent the accuracy of the TICS is indicative of the reliability of the underlying differential cross-sections. (c) 2007 Elsevier B.V. All rights reserved. C1 [Pathak, A.] Univ Hyderabad, Sch Phys, Hyderabad 500046, Andhra Pradesh, India. [Bousis, C.; Emfietzoglou, D.] Univ Ioannina, Dept Med Phys, GR-45110 Ioannina, Greece. [Hadjidoukas, P.] Univ Ioannina, Dept Comp Sci, GR-45110 Ioannina, Greece. [Nikjoo, H.] USRA, NASA Johnson Space Ctr, Ctr Adv Space Studies, Houston, TX 77058 USA. [Nikjoo, H.] Univ Nottingham, Sch Pharm, Nottingham NG7 2RD, England. [Nikjoo, H.] Univ Nottingham, Ctr Biomol Sci, Nottingham NG7 2RD, England. RP Pathak, A (reprint author), Univ Hyderabad, Sch Phys, Hyderabad 500046, Andhra Pradesh, India. EM appsp@uohyd.ernet.in RI Emfietzoglou, Dimitris/G-7168-2012; OI Hadjidoukas, Panagiotis/0000-0002-2528-7568 NR 32 TC 17 Z9 17 U1 0 U2 3 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0168-583X J9 NUCL INSTRUM METH B JI Nucl. Instrum. Methods Phys. Res. Sect. B-Beam Interact. Mater. Atoms PD APR PY 2008 VL 266 IS 8 BP 1185 EP 1192 DI 10.1016/j.nimb.2007.11.015 PG 8 WC Instruments & Instrumentation; Nuclear Science & Technology; Physics, Atomic, Molecular & Chemical; Physics, Nuclear SC Instruments & Instrumentation; Nuclear Science & Technology; Physics GA 312NH UT WOS:000256677600010 ER PT J AU Stysley, PR Poulios, D Coyle, DB Kay, RB AF Stysley, Paul R. Poulios, Demetrios Coyle, Donald B. Kay, Richard B. TI Highly efficient dual head 100 mJ TEM00 Nd : YAG oscillator SO OPTICS AND LASER TECHNOLOGY LA English DT Article DE Q-switched; Nd : YAG; LIDAR ID LASER AB A diode-pumped, Q-switched Nd:YAG laser employing a dual-pump zig-zag slab head scheme in an unstable resonator configuration for use in space-based planetary altimetry or atmospheric LIDAR is described. The pump heads are aligned orthogonally to each other, producing a symmetric overall thermal lens that eliminates the need for an intracavity cylindrical lens and aperture. This laser has demonstrated over 100 mJ in Q-switched operation with high optical efficiency (24%), good beam quality, high pointing stability, and large operational margins for multi-billion shot lifetimes. (C) 2007 Elsevier Ltd. All rights reserved. C1 [Stysley, Paul R.; Poulios, Demetrios; Kay, Richard B.] American Univ, Dept Phys, Washington, DC 20016 USA. [Coyle, Donald B.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Stysley, PR (reprint author), American Univ, Dept Phys, Washington, DC 20016 USA. EM Paul.R.Stysley@nasa.gov NR 7 TC 5 Z9 5 U1 1 U2 2 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 0030-3992 J9 OPT LASER TECHNOL JI Opt. Laser Technol. PD APR PY 2008 VL 40 IS 3 BP 435 EP 440 DI 10.1016/j.optlastec.2007.07.009 PG 6 WC Optics; Physics, Applied SC Optics; Physics GA 242TA UT WOS:000251747700002 ER PT J AU Arthur, KE Balazs, GH AF Arthur, Karen E. Balazs, George H. TI A comparison of immature green turtles (Chelonia mydas) diets among seven sites in the main Hawaiian islands' SO PACIFIC SCIENCE LA English DT Article ID SEA-TURTLES; VARIABILITY; NUMBERS; GROWTH AB Understanding resource acquisition and feeding ecology of threatened species is integral to their conservation because diet is intimately linked with growth rate and reproductive output. We examined diets of immature green sea turtles, Chelonia mnydas (L.), from seven sites on the islands of Hawai'i, O'ahu, Moloka'i, and Lana'i in January and August 2003. Diet analysis was based on 191 samples collected from 181 live green turtles by stomach lavage. These samples were identified and quantified using dissection microscopy and the principles of microstereology. Diet of green turtles in the Main Hawaiian Islands was dominated by red algae, and diet items most commonly encountered were Acanthophora spicifera (an introduced species), Hypnea sp., Pterocladiella sp., and Cladophora sp. Sea grasses (Halophila hawaiiana and H. decipiens) were an important component of diet in turtles from Kane'ohe Bay. Content of green turtle diets differed among foraging grounds, and these differences may provide an insight into previously documented differences in turtle growth rates among sites. C1 [Arthur, Karen E.] Univ Queensland, Ctr Marine Studies, St Lucia, Qld 4072, Australia. [Balazs, George H.] NOAA, Natl Marine Fisheries Serv, Pacific Isl Fisheries Sci Ctr, Honolulu, HI 96822 USA. RP Arthur, KE (reprint author), Smithsonian Marine Stn Ft Pierce, 701 Seaway Dr, Ft Pierce, FL 34949 USA. EM arthur@si.edu RI Arthur, Karen/A-3089-2012 NR 41 TC 33 Z9 36 U1 1 U2 16 PU UNIV HAWAII PRESS PI HONOLULU PA 2840 KOLOWALU ST, HONOLULU, HI 96822 USA SN 0030-8870 EI 1534-6188 J9 PAC SCI JI Pac. Sci. PD APR PY 2008 VL 62 IS 2 BP 205 EP 217 DI 10.2984/1534-6188(2008)62[205:ACOIGT]2.0.CO;2 PG 13 WC Marine & Freshwater Biology; Zoology SC Marine & Freshwater Biology; Zoology GA 287VL UT WOS:000254944500004 ER PT J AU Matsko, AB Strekalov, DV Yu, N AF Matsko, A. B. Strekalov, D. V. Yu, N. TI Sensitivity of terahertz photonic receivers SO PHYSICAL REVIEW A LA English DT Article ID FREQUENCY UP-CONVERSION; MICROWAVE RECEIVER; UPCONVERSION AB We theoretically discuss sensitivity limitations of a THz receiver which is based on up-conversion of the THz radiation into optical domain using high quality factor crystalline whispering gallery mode resonators. We show that the sensitivity of the receiver operating in the nonlinear regime approaches the sensitivity of an ideal THz photon counter. Thermal noise of the counter can be substantially reduced because of transparency of the nonlinear material in the THz frequency range. We also show that the density of power fluctuations of the receiver operating in the linear regime is given by the THz shot noise. C1 [Matsko, A. B.; Strekalov, D. V.; Yu, N.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Matsko, AB (reprint author), OEwaves Inc, 1010 E Union St, Pasadena, CA 91106 USA. NR 13 TC 12 Z9 12 U1 0 U2 2 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 1050-2947 J9 PHYS REV A JI Phys. Rev. A PD APR PY 2008 VL 77 IS 4 AR 043812 DI 10.1103/PhysRevA.77.043812 PG 5 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA 295EF UT WOS:000255457100168 ER PT J AU Boykin, TB Luisier, M Klimeck, G AF Boykin, Timothy B. Luisier, Mathieu Klimeck, Gerhard TI Multiband transmission calculations for nanowires using an optimized renormalization method SO PHYSICAL REVIEW B LA English DT Article ID SYSTEMS; SEMICONDUCTORS; TRANSPORT; DEVICES; MODEL AB The discovery of an interesting nanostructure behavior or the design of useful nanodevices requires state-of-the-art physical models. Realistic, multiband nanowire calculations especially tend to be computationally intensive and slow. Here, we develop optimizations to the renormalization method of Grosso [Phys. Rev. B 40, 12328 (1989)] specifically for nanowires with [100]- or [111]-oriented axes. For no-spin-orbit models, our optimizations give far superior performance to other available methods, while for spin-orbit models on a single processor, our results are at least as good as the best alternative. More importantly, the parallel scalability of our optimizations is superior to that of other available methods, making optimized renormalization very attractive for multiple-processor computers. We demonstrate the method with calculations for Si nanowires. C1 [Boykin, Timothy B.] Univ Alabama, Dept Elect & Comp Engn, Huntsville, AL 35899 USA. [Luisier, Mathieu] ETH, Integrated Syst Lab, CH-8092 Zurich, Switzerland. [Klimeck, Gerhard] Purdue Univ, Sch Elect & Comp Engn, Network Computat Nanotechnol, 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. RI Klimeck, Gerhard/A-1414-2012 OI Klimeck, Gerhard/0000-0001-7128-773X NR 19 TC 13 Z9 13 U1 0 U2 5 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 1098-0121 J9 PHYS REV B JI Phys. Rev. B PD APR PY 2008 VL 77 IS 16 AR 165318 DI 10.1103/PhysRevB.77.165318 PG 9 WC Physics, Condensed Matter SC Physics GA 295EJ UT WOS:000255457500075 ER PT J AU Cantrell, JH Cantrell, SA AF Cantrell, John H. Cantrell, Sean A. TI Analytical model of the nonlinear dynamics of cantilever tip-sample surface interactions for various acoustic atomic force microscopies SO PHYSICAL REVIEW B LA English DT Article ID TAPPING-MODE; VIBRATIONS; BEAM AB An analytical model is developed of the interaction of the cantilever tip of an atomic force microscope with the sample surface that treats the cantilever and sample as independent systems coupled by a nonlinear force acting between the cantilever tip and a volume element of the sample surface. To maintain equilibrium, the volume element is subjected to a restoring force from the remainder of the sample. The model accounts for the positions on the cantilever of the cantilever tip, laser probe, and excitation force (if any). The model leads to a pair of coupled nonlinear differential equations that are solved analytically using a matrix iteration procedure. Solutions are obtained for the phase and amplitude signals generated by various acoustic atomic force microscope (A-AFM) techniques including force modulation microscopy, atomic force acoustic microscopy, ultrasonic force microscopy, heterodyne force microscopy, resonant difference-frequency atomic force ultrasonic microscopy (RDF-AFUM), and amplitude modulation-atomic force microscopy (AM-AFM) (intermittent contact mode). The solutions are used to obtain a quantitative measure of A-AFM image contrast resulting from variations in the Young modulus of the sample. Applications of the model to measurements of LaRC (TM)-CP2 polyimide film using RDF-AFUM and AM-AFM images predict maximum variations in the Young modulus of 24% and 18%, respectively, over a common scan area. Both predictions are in good agreement with the value of 21% obtained from independent mechanical stretching measurements of the polyimide sheet material. C1 [Cantrell, John H.] NASA, Langley Res Ctr, Hampton, VA 23681 USA. [Cantrell, Sean A.] Univ Virginia, Dept Phys, Charlottesville, VA 22901 USA. RP Cantrell, JH (reprint author), NASA, Langley Res Ctr, Mail Stop 231, Hampton, VA 23681 USA. EM john.h.cantrell@nasa.gov; sac3k@virginia.edu NR 41 TC 19 Z9 19 U1 1 U2 20 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 2469-9950 EI 2469-9969 J9 PHYS REV B JI Phys. Rev. B PD APR PY 2008 VL 77 IS 16 AR 165409 DI 10.1103/PhysRevB.77.165409 PG 16 WC Physics, Condensed Matter SC Physics GA 295EJ UT WOS:000255457500107 ER PT J AU Lawson, JW Srivastava, D AF Lawson, John W. Srivastava, Deepak TI Formation and structure of amorphous carbon char from polymer materials SO PHYSICAL REVIEW B LA English DT Article ID FLAMMABILITY PROPERTIES; NANOCOMPOSITES; COMPOSITES AB Amorphous carbonaceous char produced from burning polymer solids has insulating properties that make it valuable in thermal protection and fire-retardant systems. A pyrolytic molecular dynamics simulation method is devised to study the transformation of the local microstructure from virgin polymer to a dense, disordered char. Release of polymer hydrogen is found to be critical to allow the system to collapse into a highly coordinated char structure. Mechanisms of the char formation process and the morphology of the resulting structures are elucidated. C1 [Lawson, John W.; Srivastava, Deepak] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Lawson, JW (reprint author), NASA, Ames Res Ctr, Mail Stop 269-2, Moffett Field, CA 94035 USA. EM john.w.lawson@nasa.gov; dsrivastava@mail.arc.nasa.gov NR 16 TC 16 Z9 16 U1 0 U2 14 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 1098-0121 J9 PHYS REV B JI Phys. Rev. B PD APR PY 2008 VL 77 IS 14 AR 144209 DI 10.1103/PhysRevB.77.144209 PG 6 WC Physics, Condensed Matter SC Physics GA 295EH UT WOS:000255457300033 ER PT J AU Berti, E Cardoso, V AF Berti, Emanuele Cardoso, Vitor TI Quasinormal modes and thermodynamic phase transitions SO PHYSICAL REVIEW D LA English DT Article ID BLACK-HOLES AB It has recently been suggested that scalar, Dirac, and Rarita-Schwinger perturbations are related to thermodynamic phase transitions of charged (Reissner-Nordstrom) black holes. In this Brief Report we show that this result is probably a numerical coincidence, and that the conjectured correspondence does not straightforwardly generalize to other metrics, such as Kerr or Schwarzschild (anti-)de Sitter. Our calculations do not rule out a relation between dynamical and thermodynamical properties of black holes, but they suggest that such a relation is nontrivial. C1 [Berti, Emanuele] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Cardoso, Vitor] Inst Super Tecn, Dept Fis, Ctr Multidisciplinar Astrofis CENTRA, P-1049001 Lisbon, Portugal. [Cardoso, Vitor] Univ Mississippi, Dept Phys & Astron, University, MS 38677 USA. RP Berti, E (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM berti@wugrav.wustl.edu; vcardoso@fisica.ist.utl.pt RI Berti, Emilio/F-5256-2012; Berti, Emanuele/C-9331-2016; Cardoso, Vitor/K-1877-2015 OI Berti, Emanuele/0000-0003-0751-5130; Cardoso, Vitor/0000-0003-0553-0433 NR 25 TC 13 Z9 13 U1 0 U2 2 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 1550-7998 J9 PHYS REV D JI Phys. Rev. D PD APR PY 2008 VL 77 IS 8 AR 087501 DI 10.1103/PhysRevD.77.087501 PG 4 WC Astronomy & Astrophysics; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA 295EN UT WOS:000255457900091 ER PT J AU Umstatter, R Tinto, M AF Umstaetter, Richard Tinto, Massimo TI Bayesian comparison of post-Newtonian approximations of gravitational wave chirp signals SO PHYSICAL REVIEW D LA English DT Article ID MODEL AB We estimate the probability of detecting a gravitational wave signal from coalescing compact binaries in simulated data from a ground-based interferometer detector of gravitational radiation using Bayesian model selection. The simulated wave form of the chirp signal is assumed to be a spinless post-Newtonian (PN) wave form of a given expansion order, while the searching template is assumed to be either of the same post-Newtonian family as the simulated signal or one level below its post-Newtonian expansion order. Within the Bayesian framework, and by applying a reversible jump Markov Chain Monte Carlo simulation algorithm, we compare PN1.5 vs PN2.0 and PN3.0 vs PN3.5 wave forms by deriving the detection probabilities, the statistical uncertainties due to noise as a function of the signal-to-noise ratio, and the posterior distributions of the parameters. Our analysis indicates that the detection probabilities are not compromised when simplified models are used for the comparison, while the accuracies in the determination of the parameters characterizing these signals can be significantly worsened, no matter what the considered post-Newtonian order expansion comparison is. C1 [Umstaetter, Richard; Tinto, Massimo] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Umstaetter, Richard; Tinto, Massimo] CALTECH, LIGO Labs, Pasadena, CA 91125 USA. RP Umstatter, R (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM richard.umstaetter@jpl.nasa.gov; massimo.tinto@jpl.nasa.gov NR 37 TC 7 Z9 7 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 APR PY 2008 VL 77 IS 8 AR 082002 DI 10.1103/PhysRevD.77.082002 PG 19 WC Astronomy & Astrophysics; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA 295EN UT WOS:000255457900004 ER PT J AU Berg, RF Moldover, MR Yao, MW Zimmerli, GA AF Berg, Robert F. Moldover, Michael R. Yao, Minwu Zimmerli, Gregory A. TI Shear thinning near the critical point of xenon SO PHYSICAL REVIEW E LA English DT Article ID CRITICAL FLUIDS; DROPLET MODEL; TRANSPORT-PROPERTIES; MICELLAR-SOLUTION; VISCOSITY; FLOW; TEMPERATURE; WATER; MIXTURES; DYNAMICS AB We measured shear thinning, a viscosity decrease ordinarily associated with complex liquids, near the critical point of xenon. The data span a wide range of reduced shear rate: 10(-3) (gamma) over dot tau < 700, where (gamma) over dot tau is the shear rate scaled by the relaxation time tau of critical fluctuations. The measurements had a temperature resolution of 0.01 mK and were conducted in microgravity aboard the Space Shuttle Columbia to avoid the density stratification caused by Earth's gravity. The viscometer measured the drag on a delicate nickel screen as it oscillated in the xenon at amplitudes 3 mu m < x(0) < 430 mu m and frequencies 1 Hz < omega/2 pi < 5 Hz. To separate shear thinning from other nonlinearities, we computed the ratio of the viscous force on the screen at (gamma) over dot tau to the force at (gamma) over dot tau approximate to 0: C(gamma) F(x(0), omega tau, (gamma) over dot tau)/F (x(0), omega tau, 0). At low frequencies, (omega tau)(2) < (gamma) over dot tau, C(gamma) depends only on (gamma) over dot tau, as predicted by dynamic critical scaling. At high frequencies, (omega tau)(2) > (gamma) over dot tau, C gamma depends also on both x(0) and omega. The data were compared with numerical calculations based on the Carreau-Yasuda relation for complex fluids: eta((gamma) over dot)/ eta(0) = [1 + A(gamma)|(gamma) over dot tau|](-x eta/(3+x eta)), where x eta = 0.069 is the critical exponent for viscosity and mode-coupling theory predicts A(gamma)= 0.121. For xenon we find A(gamma) = 0.137 +/- 0.029, in agreement with the mode coupling value. Remarkably, the xenon data close to the critical temperature T(c) were independent of the cooling rate (both above and below T(c)) and these data were symmetric about T(c) to within a temperature scale factor. The scale factors for the magnitude of the oscillator's response differed from those for the oscillator's phase; this suggests that the surface tension of the two-phase domains affected the drag on the screen below T(c). C1 [Berg, Robert F.; Moldover, Michael R.] Natl Inst Stand & Technol, Gaithersburg, MD 20899 USA. [Yao, Minwu] Ohio Aerosp Inst, Cleveland, OH 44142 USA. [Zimmerli, Gregory A.] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. RP Berg, RF (reprint author), Natl Inst Stand & Technol, Gaithersburg, MD 20899 USA. RI Moldover, Michael/E-6384-2013 NR 51 TC 5 Z9 5 U1 1 U2 6 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 1539-3755 J9 PHYS REV E JI Phys. Rev. E PD APR PY 2008 VL 77 IS 4 AR 041116 DI 10.1103/PhysRevE.77.041116 PN 1 PG 23 WC Physics, Fluids & Plasmas; Physics, Mathematical SC Physics GA 295ED UT WOS:000255456900019 PM 18517587 ER PT J AU Schindler, K Hesse, M AF Schindler, Karl Hesse, Michael TI Formation of thin bifurcated current sheets by quasisteady compression SO PHYSICS OF PLASMAS LA English DT Article ID COLLISIONLESS MAGNETIC RECONNECTION; ELECTRIC-CURRENT SHEET; SUBSTORM GROWTH-PHASE; PLASMA SHEET; MAGNETOTAIL; FIELD AB Thin current sheets with half-widths in the range of about 10 or less ion inertial lengths (or ion gyroradii) have been identified as the sites of important dynamical phenomena in space plasmas. Recent space observations established that thin current sheets often have a bifurcated (double-peaked) current density. Earlier suggestions of possible bifurcation mechanisms are based on the presence of microfluctuations, magnetic reconnection, or a normal magnetic field component or assumed simplified models of adiabatic dynamics. Despite these efforts, the cause (or causes) of the formation of thin bifurcated current sheets and the conditions under which they form have remained unclear. In this paper, we identify quasisteady compression of a plane, initially wide collisionless current sheet as an effective physical mechanism for the formation of thin bifurcated current sheets. Our main tool is electromagnetic particle simulation. The initial sheet has a singly peaked current and a half-width that is five times larger than the ion inertial length. This sheet is quasisteadily compressed by external forces. A three-scale structure develops and the current bifurcates during compression. It is shown that the bifurcation, pressure anisotropy, and other major properties of the embedded current sheet can be understood in terms of basic physical principles, such as electric field shielding and momentum conservation. Sufficient conditions for bifurcation of symmetric current sheets are presented. They suggest that bifurcation must generally occur by quasisteady compression if the (singly peaked) initial current sheet is sufficiently wide. (c) 2008 American Institute of Physics. C1 [Schindler, Karl] Ruhr Univ Bochum, D-44780 Bochum, Germany. [Hesse, Michael] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Schindler, K (reprint author), Ruhr Univ Bochum, D-44780 Bochum, Germany. RI Hesse, Michael/D-2031-2012; NASA MMS, Science Team/J-5393-2013 OI NASA MMS, Science Team/0000-0002-9504-5214 NR 40 TC 12 Z9 12 U1 0 U2 1 PU AMER INST PHYSICS PI MELVILLE PA CIRCULATION & FULFILLMENT DIV, 2 HUNTINGTON QUADRANGLE, STE 1 N O 1, MELVILLE, NY 11747-4501 USA SN 1070-664X J9 PHYS PLASMAS JI Phys. Plasmas PD APR PY 2008 VL 15 IS 4 AR 042902 DI 10.1063/1.2907359 PG 9 WC Physics, Fluids & Plasmas SC Physics GA 295EB UT WOS:000255456700044 ER PT J AU Zenitani, S Hesse, M AF Zenitani, S. Hesse, M. TI The role of the Weibel instability at the reconnection jet front in relativistic pair plasma reconnection (vol 15, art no 022101, 2008) SO PHYSICS OF PLASMAS LA English DT Correction C1 [Zenitani, S.; Hesse, M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Zenitani, S (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. EM zenitani@lssp-mail.gsfc.nasa.gov RI Hesse, Michael/D-2031-2012; NASA MMS, Science Team/J-5393-2013 OI NASA MMS, Science Team/0000-0002-9504-5214 NR 1 TC 0 Z9 0 U1 0 U2 0 PU AMER INST PHYSICS PI MELVILLE PA CIRCULATION & FULFILLMENT DIV, 2 HUNTINGTON QUADRANGLE, STE 1 N O 1, MELVILLE, NY 11747-4501 USA SN 1070-664X J9 PHYS PLASMAS JI Phys. Plasmas PD APR PY 2008 VL 15 IS 4 AR 049901 DI 10.1063/1.2891088 PG 1 WC Physics, Fluids & Plasmas SC Physics GA 295EB UT WOS:000255456700061 ER PT J AU Tomasko, MG Doose, L Engel, S Dafoe, LE West, R Lemmon, M Karkoschka, E See, C AF Tomasko, M. G. Doose, L. Engel, S. Dafoe, L. E. West, R. Lemmon, M. Karkoschka, E. See, C. TI A model of Titan's aerosols based on measurements made inside the atmosphere SO PLANETARY AND SPACE SCIENCE LA English DT Article DE Titan; aerosols; Huygens; atmosphere ID T-MATRIX; SCATTERING; PARTICLES; DESCENT; SPHERES; WAVELENGTH; PROBE; HAZE AB The descent imager/spectral radiometer (DISR) instrument aboard the Huygens probe into the atmosphere of Titan measured the brightness of sunlight using a complement of spectrometers, photometers, and cameras that covered the spectral range from 350 to 1600 nm, looked both upward and downward, and made measurements at altitudes from 150 km to the surface. Measurements from the upward-looking visible and infrared spectrometers are described in Tomasko et al. [2008a. Measurements of methane absorption by the descent imager/spectral radiometer (DISR) during its descent through Titan's atmosphere. Planet. Space Sci., this volume]. Here, we very briefly review the measurements by the violet photometers, the downward-looking visible and infrared spectrometers, and the upward-looking solar aureole (SA) camera. Taken together, the DISR measurements constrain the vertical distribution and wavelength dependence of opacity, single-scattering albedo, and phase function of the aerosols in Titan's atmosphere. Comparison of the inferred aerosol properties with computations of scattering from fractal aggregate particles indicates the size and shape of the aerosols. We find that the aggregates require monomers of radius 0.05 mu m or smaller and that the number of monomers in the loose aggregates is roughly 3000 above 60 km. The single-scattering albedo, of the aerosols above 140 kin altitude is similar to that predicted for some tholins measured in laboratory experiments, although we find that the single-scattering albedo of the aerosols increases with depth into the atmosphere between 140 and 80km altitude, possibly due to condensation of other gases on the haze particles. The number density of aerosols is about 5/cm(3) at 80 km altitude, and decreases with a scale height of 65 km to higher altitudes. The aerosol opacity above 80 km varies as the wavelength to the -2.34 power between 350 and 1600 nm. Between 80 and 30 km the cumulative aerosol opacity increases linearly with increasing depth in the atmosphere. The total aerosol opacity in this altitude range varies as the wavelength to the -1.41 power. The single-scattering phase function of the aerosols in this region is also consistent with the fractal particles found above 60 km. In the lower 30 km of the atmosphere, the wavelength dependence of the aerosol opacity varies as the wavelength to the -0.97 power, much less than at higher altitudes. This suggests that the aerosols here grow to still larger sizes, possibly by incorporation of methane into the aerosols. Here the cumulative opacity also increases linearly with depth, but at some wavelengths the rate is slightly different than above 30 km altitude. For purely fractal particles in the lowest few km, the intensity looking upward opposite to the azimuth of the sun decreases with increasing zenith angle faster than the observations in red light if the single-scattering albedo is assumed constant with altitude at these low altitudes. This discrepancy can be decreased if the single-scattering albedo decreases with altitude in this region. A possible explanation is that the brightest aerosols near 30 km altitude contain significant amounts of methane, and that the decreasing albedo at lower altitudes may reflect the evaporation of some of the methane as the aerosols fall into dryer layers of the atmosphere. An alternative explanation is that there may be spherical particles in the bottom few kilometers of the atmosphere. Published by Elsevier Ltd. C1 [Tomasko, M. G.; Doose, L.; Engel, S.; Dafoe, L. E.; Karkoschka, E.; See, C.] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA. [West, R.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Lemmon, M.] Texas A&M Univ, Dept Atmospher Sci, College Stn, TX 77843 USA. RP Tomasko, MG (reprint author), Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA. EM mtomasko@lpl.arizona.edu RI Lemmon, Mark/E-9983-2010 OI Lemmon, Mark/0000-0002-4504-5136 NR 20 TC 130 Z9 130 U1 3 U2 23 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0032-0633 J9 PLANET SPACE SCI JI Planet Space Sci. PD APR PY 2008 VL 56 IS 5 BP 669 EP 707 DI 10.1016/j.pss.2007.11.019 PG 39 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 296VS UT WOS:000255574500009 ER PT J AU Witasse, O Huber, L Zender, J Lebreton, JP Beebe, R Heather, D Matson, DL Zarnecki, J Wheadon, J Trautner, R Tomasko, M Stoppato, PL Simoes, F See, C Perez-Ayucar, M Pennanech, C Niemann, H McFarlane, L Leese, M Kazeminejad, B Israel, G Hathi, B Hagermann, A Haberman, J Fulchignoni, M Ferri, F Dutta-Roy, R Doose, L Demick-Montelara, J Colombatti, G Brun, JF Bird, M Atkinson, D Aboudan, A AF Witasse, Olivier Huber, Lyle Zender, Joe Lebreton, Jean-Pierre Beebe, Reta Heather, David Matson, Dennis L. Zarnecki, John Wheadon, Joe Trautner, Roland Tomasko, Marty Stoppato, Piero Leon Simoes, Fernando See, Chuck Perez-Ayucar, Miguel Pennanech, Cyril Niemann, Hasso McFarlane, Lisa Leese, Mark Kazeminejad, Bobby Israel, Guy Hathi, Brijen Hagermann, Axel Haberman, John Fulchignoni, Marcello Ferri, Francesca Dutta-Roy, Robindro Doose, Lyn Demick-Montelara, Jaime Colombatti, Giacomo Brun, Jean-Francis Bird, Michael Atkinson, David Aboudan, Alessio TI The Huygens scientific data archive: Technical overview SO PLANETARY AND SPACE SCIENCE LA English DT Article DE Cassini/Huygens mission; data archiving; Titan ID TITAN; DESCENT; SURFACE; WINDS; PROBE AB The Cassini/Huygens. mission was launched in October 1997, and during the third orbit around Saturn, the Huygens probe was released on course to enter Titan's atmosphere. During the descent, six science instruments provided in situ and remote sensing measurements of Titan's atmosphere and surface. Doppler tracking was performed with two Earth-based radio telescopes, and a Very Long Base Interferometry (VLBI) experiment was carried out. Data acquisition began around 1500 km altitude and continued throughout the 2 h and 30 min descent and for 1 h and 12 min after landing. This unique set of data is available in the ESA Planetary Science Archive (PSA) and mirror imaged in the NASA Planetary Data System (PDS). This paper presents an overview of the process the Huygens Data Archiving Working Group followed to develop and ingest the data set. A description of the data sets is also given. (C) 2007 Elsevier Ltd. All rights reserved. C1 [Witasse, Olivier; Zender, Joe; Lebreton, Jean-Pierre; Heather, David; Trautner, Roland; Perez-Ayucar, Miguel] European Space Agcy, Res & Sci Support Dept, ESTEC, NL-2200 AG Noordwijk, Netherlands. [Huber, Lyle; Beebe, Reta] New Mexico State Univ, Dept Astron, Las Cruces, NM 88003 USA. [Matson, Dennis L.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Zarnecki, John; Leese, Mark; Hathi, Brijen; Hagermann, Axel] Open Univ, Planetary & Space Sci Res Inst, Milton Keynes MK7 6AA, Bucks, England. [Wheadon, Joe] ESOC, ESA, D-64293 Darmstadt, Germany. [Tomasko, Marty; See, Chuck; McFarlane, Lisa; Doose, Lyn] Kuiper LPL, Tucson, AZ 85721 USA. [Stoppato, Piero Leon; Ferri, Francesca; Colombatti, Giacomo; Aboudan, Alessio] Univ Padua, CISAS G Colombo, I-35131 Padua, Italy. [Pennanech, Cyril; Brun, Jean-Francis] CNRS, Serv Aeron, F-91371 Verrieres Le Buisson, France. [Niemann, Hasso; Haberman, John; Demick-Montelara, Jaime] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20117 USA. [Kazeminejad, Bobby] GSOC, Deutsch Zentrum Luft & Raumfahrt, D-82234 Wesssling, Germany. [Fulchignoni, Marcello] Observ Paris, LESIA, F-92195 Meudon, France. [Dutta-Roy, Robindro; Bird, Michael] Univ Bonn, Argelander Inst Astron, D-53121 Bonn, Germany. [Atkinson, David] Univ Idaho, Dept Elect & Comp Engn, Moscow, ID 83844 USA. [Simoes, Fernando] IPSL CNRS, CETP, F-94107 St Maur, France. RP Witasse, O (reprint author), European Space Agcy, Res & Sci Support Dept, ESTEC, NL-2200 AG Noordwijk, Netherlands. EM owitasse@rssd.esa.int RI Simoes, Fernando/D-7731-2012 NR 7 TC 1 Z9 1 U1 0 U2 6 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0032-0633 J9 PLANET SPACE SCI JI Planet Space Sci. PD APR PY 2008 VL 56 IS 5 BP 770 EP 777 DI 10.1016/j.pss.2007.10.007 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 296VS UT WOS:000255574500014 ER PT J AU Gillespie, TW Foody, GM Rocchini, D Giorgi, AP Saatchi, S AF Gillespie, Thomas W. Foody, Giles M. Rocchini, Duccio Giorgi, Ana Paula Saatchi, Sassan TI Measuring and modelling biodiversity from space SO PROGRESS IN PHYSICAL GEOGRAPHY LA English DT Review DE biogeography; conservation planning; diversity modelling; remote sensing; species distribution modelling ID PLANT-SPECIES RICHNESS; RESOLUTION SATELLITE DATA; LAND-COVER CLASSIFICATION; REGIONAL-SCALE ANALYSIS; TROPICAL RAIN-FORESTS; REMOTELY-SENSED DATA; SPATIAL-RESOLUTION; SPECTRAL-RESOLUTION; BETA-DIVERSITY; CONSERVATION PRIORITIES AB The Earth is undergoing an accelerated rate of native ecosystem conversion and degradation and there is increased interest in measuring and modelling biodiversity from space. Biogeographers have a long-standing interest in measuring patterns of species occurrence and distributional movements and an interest in modelling species distributions and patterns of diversity. Much progress has been made in identifying plant species from space using high-resolution satellites (QuickBird, IKONOS), while the measurement of species movements has become commonplace with the ARGOS satellite tracking system which has been used to track the movements of thousands of individual animals. There have been significant advances in land-cover classifications by combining data from multi-passive and active sensors, and new classification techniques. Species distribution modelling has been growing at a striking rate and the incorporation of spaceborne data on climate, topography, land cover, and vegetation structure has great potential to improve models. There have been significant advances in modelling species richness, alpha diversity, and beta diversity using multisensors to quantify land-cover classifications and landscape metrics, measures of productivity, and measures of heterogeneity. Remote sensing of nature reserves can provide natural resources managers with near real-time data within and around reserves that can be used to support conservation efforts anywhere in the world. Future research should focus on incorporating recent spaceborne sensors, more extensive integration of available spaceborne imagery, and the collection and dissemination of high-quality field data. This will improve our understanding of the distribution of life on earth. C1 [Gillespie, Thomas W.; Giorgi, Ana Paula] Univ Calif Los Angeles, Dept Geog, Los Angeles, CA 90095 USA. [Foody, Giles M.] Univ Nottingham, Sch Geog, Nottingham NG7 2RD, England. [Rocchini, Duccio] Univ Siena, Dipartimento Sci Ambientali G Sarfatti, I-53100 Siena, Italy. [Saatchi, Sassan] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Gillespie, TW (reprint author), Univ Calif Los Angeles, Dept Geog, Los Angeles, CA 90095 USA. EM tg@geog.ucla.edu RI Rocchini, Duccio/B-6742-2011; OI Rocchini, Duccio/0000-0003-0087-0594 NR 147 TC 163 Z9 174 U1 9 U2 79 PU SAGE PUBLICATIONS LTD PI LONDON PA 1 OLIVERS YARD, 55 CITY ROAD, LONDON EC1Y 1SP, ENGLAND SN 0309-1333 J9 PROG PHYS GEOG JI Prog. Phys. Geogr. PD APR PY 2008 VL 32 IS 2 BP 203 EP 221 DI 10.1177/0309133308093606 PG 19 WC Geography, Physical; Geosciences, Multidisciplinary SC Physical Geography; Geology GA 345IG UT WOS:000258989200004 ER PT J AU Bauer, JM Choi, YJ Weissman, PR Stansberry, JA Fernandez, YR Roe, HG Buratti, BJ Sung, HI AF Bauer, James M. Choi, Young-Jun Weissman, Paul R. Stansberry, John A. Fernandez, Yanga R. Roe, Henry G. Buratti, Bonnie J. Sung, Hyun-Il TI The large-grained dust coma of 174P/Echeclus SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF THE PACIFIC LA English DT Article ID SPITZER-SPACE-TELESCOPE; DEEP-IMPACT; ABSOLUTE CALIBRATION; INFRARED PHOTOMETRY; HALE-BOPP; COMETS; CENTAURS; NUCLEUS; OBJECTS; 2060-CHIRON AB On 2005 December 30, Y.- J. Choi and P. R. Weissman discovered that the formerly dormant Centaur 2000 EC98 was in strong outburst. Previous observations by P. Rousselot et al. spanning a 3-year period indicated a lack of coma down to the 27 mag arcsec(-2) level. We present Spitzer Space Telescope MIPS observations of this newly active Centaur - now known as 174P/Echeclus ( 2000 EC98) - or 60558 Echeclus - taken in 2006 late February. The images show strong signal at both the 24 and 70 mu m bands and reveal an extended coma about 2' in diameter. Analyses yield estimates of the coma signal contribution that are in excess of 90% of the total signal in the 24 mu m band. Dust production estimates ranging from 1.7 - 4 x 10(2) kg s(-1) are on the order of 30 times that seen in other Centaurs. Simultaneous visible-wavelength observations were also obtained with Palomar Observatory's 200-inch telescope, the 1.8-m Vatican Advanced Technology Telescope, the Bohyunsan Optical Astronomy Observatory (BOAO) 1.8-m telescope, and Table Mountain Observatory's 0.6-m telescope, revealing a coma morphology nearly identical to the mid-IR observations. The grain size distribution derived from the data yields a log particle mass power-law with slope parameter alpha = -0.87 +/- 0.07, and is consistent with steady cometary activity, such as that observed during the Stardust spacecraft's encounter at 81P/Wild 2, and not with an impact-driven event, such as that caused by the Deep Impact experiment. C1 [Bauer, James M.; Choi, Young-Jun; Weissman, Paul R.; Buratti, Bonnie J.] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Stansberry, John A.] Univ Arizona, Steward Observ, Tucson, AZ USA. [Fernandez, Yanga R.] Univ Cent Florida, Dept Phys, Orlando, FL USA. [Roe, Henry G.] Lowell Observ, Flagstaff, AZ 86001 USA. [Sung, Hyun-Il] Korea Astron & Space Sci Inst, Taejon 305348, South Korea. RP Bauer, JM (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA USA. OI Fernandez, Yanga/0000-0003-1156-9721 NR 55 TC 17 Z9 17 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-6280 J9 PUBL ASTRON SOC PAC JI Publ. Astron. Soc. Pac. PD APR PY 2008 VL 120 IS 866 BP 393 EP 404 DI 10.1086/587552 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 290KF UT WOS:000255121000005 ER PT J AU Chuss, DT Wollack, EJ Moseley, SH Withington, S Saklatvala, G AF Chuss, David T. Wollack, Edward J. Moseley, S. Harvey Withington, Stafford Saklatvala, George TI Diffraction considerations for planar detectors in the few-mode limit SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF THE PACIFIC LA English DT Article ID TELESCOPE; ARRAYS; CAMERA AB Filled arrays of bolometers are currently being employed for use in astronomy from the far-infrared through millimeter portion of the electromagnetic spectrum. Because of the large range of wavelengths for which such detectors are applicable, the size of a pixel (p) relative to the wavelength (lambda) will vary according to the specific application of a given available technology. As the pixel size becomes comparable to a wavelength of the absorbed radiation, correlations in the radiation field at the pixel can affect the imaging properties of the system independent of the correlations introduced by the front-end optics. We study the dependence of image fidelity and induced polarization on the size of the pixel by employing a formalism in which diffraction due to the pixel boundary is treated by propagating the second-order statistical correlations of the radiation field through an optical system. We construct simulated polarized images of square pixels for various ratios of p/lambda. For the limit in which few modes are supported by the pixel (p/lambda less than or similar to 1), we find that the diffraction due to the pixel edges is nonnegligible and hence must be considered along with the telescope diffraction pattern in modeling the ultimate spatial resolution of an imaging system. For the case in which the pixel is over-moded (p/lambda >> 1), the geometric limit is approached as expected. This technique provides a quantitative approach to understand and optimize the imaging properties of planar detectors in the few-mode limit. C1 [Chuss, David T.; Wollack, Edward J.; Moseley, S. Harvey] NASA, Goddard Space Flight Ctr, Observat Cosmol Lab, Greenbelt, MD USA. [Withington, Stafford; Saklatvala, George] Univ Cambridge, Cavevdish Lab, Cambridge CB3 OHE, England. RP Chuss, DT (reprint author), NASA, Goddard Space Flight Ctr, Observat Cosmol Lab, Code 665, Greenbelt, MD USA. EM David.T.Chuss@nasa.gov; Edward.J.Wollack@nasa.gov; Harvey.Moseley@nasa.gov; stafford@mrao.cam.ac.uk RI Moseley, Harvey/D-5069-2012; Chuss, David/D-8281-2012; Wollack, Edward/D-4467-2012 OI Wollack, Edward/0000-0002-7567-4451 NR 13 TC 10 Z9 10 U1 0 U2 2 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-6280 J9 PUBL ASTRON SOC PAC JI Publ. Astron. Soc. Pac. PD APR PY 2008 VL 120 IS 866 BP 430 EP 438 DI 10.1086/587494 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 290KF UT WOS:000255121000008 ER PT J AU Weinstein, SA Lundgren, PR AF Weinstein, Stuart A. Lundgren, Paul R. TI Finite fault modeling in a tsunami warning center context SO PURE AND APPLIED GEOPHYSICS LA English DT Article DE Finite fault modeling; earthquake rupture history; tsunami warning center ID STRONG-MOTION; MANTLE MAGNITUDE; RUPTURE HISTORY; EARTHQUAKE; INVERSION; CALIFORNIA; RECORDS; WAVES AB The US NOAA/NWS tsunami warning centers have relied on earthquake location and depth, and scalar measures of earthquake size and slowness to assess the potential for the generation of a destructive tsunami by an earthquake. Recent earthquakes, such as Peru 2001, Sumatra 2004 and the Java 2006, manifest some of the difficulties the warning centers face as they try to cope with unusual earthquakes. We have undertaken a study of a simple teleseismic waveform inverse model and applied it to the earthquakes of June 23, 2001 in Peru and of July 17, 2006 in Java. Synthetic numerical experiments suggest that the most salient features of the rupture history of an earthquake can be recovered. Furthermore the calculations can be conducted quickly enough to be useful in a warning center context. We have applied our technique to the Peru 2001 and recent Java 2006 earthquakes. Our overall results are consistent with those obtained from other studies. The results show why the Peru event initially looked slow to the US tsunami warning centers and that the Java event is a truly slow or tsunami earthquake. Clearly, the warning centers stand to benefit from an increased understanding of the earthquakes they monitor. Furthermore, better knowledge of the slip distribution along a fault will improve tsunami wave-height forecasts. C1 [Weinstein, Stuart A.] Richard H Hagemeyers Pacific Tsunami Warning Ctr, Ewa Beach, HI 96706 USA. [Lundgren, Paul R.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Weinstein, SA (reprint author), Richard H Hagemeyers Pacific Tsunami Warning Ctr, Ewa Beach, HI 96706 USA. EM stuart.weinstein@noaa.gov NR 21 TC 5 Z9 5 U1 0 U2 1 PU SPRINGER BASEL AG PI BASEL PA PICASSOPLATZ 4, BASEL, 4052, SWITZERLAND SN 0033-4553 EI 1420-9136 J9 PURE APPL GEOPHYS JI Pure Appl. Geophys. PD APR PY 2008 VL 165 IS 3-4 BP 451 EP 474 DI 10.1007/s00024-008-0316-x PG 24 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 301AA UT WOS:000255867100002 ER PT J AU Parker, J Lyzenga, G Norton, C Zuffada, C Glasscoe, M Lou, J Donnellan, A AF Parker, Jay Lyzenga, Gregory Norton, Charles Zuffada, Cinzia Glasscoe, Margaret Lou, John Donnellan, Andrea TI Geophysical finite-element simulation tool (GeoFEST): Algorithms and validation for quasistatic regional faulted crust problems SO PURE AND APPLIED GEOPHYSICS LA English DT Article AB GeoFEST (Geophysical Finite Element Simulation Tool) is a two- and three-dimensional finite element software package for the modeling of solid stress and strain in geophysical and other continuum domain applications. It is one of the featured high-performance applications of the NASA QuakeSim project. The program is targeted to be compiled and run on UNIX systems, and is running on diverse systems including sequential and message-passing parallel systems. Solution to the elliptical partial differential equations is obtained by finite element basis sampling, resulting in a sparse linear system primarily solved by conjugate gradient iteration to a tolerance level; on sequential systems a Crout factorization for the direct inversion of the linear system is also supported. The physics models supported include isotropic linear elasticity and both Newtonian and power-law viscoelasticity, via implicit quasi-static time stepping. In addition to triangular, quadrilateral, tetrahedral and hexahedral continuum elements, GeoFEST supports split-node faulting, body forces, and surface tractions. This software and related mesh refinement strategies have been validated on a variety of test cases with rigorous comparison to analytical solutions. These include a box-shaped domain with imposed motion on one surface, a pair of strike slip faults in stepover arrangement, and two community-agreed benchmark cases: a strike slip fault in an enclosing box, and a quarter-domain circular fault problem. Scientific applications of the code include the modeling of static and transient co- and post-seismic earth deformation, Earth response to glacial, atmospheric and hydrological loading, and other scenarios involving the bulk deformation of geologic media. C1 [Parker, Jay; Lyzenga, Gregory; Norton, Charles; Zuffada, Cinzia; Glasscoe, Margaret; Lou, John; Donnellan, Andrea] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Parker, J (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM Jay.W.Parker@jpl.nasa.gov NR 12 TC 7 Z9 7 U1 0 U2 1 PU BIRKHAUSER VERLAG AG PI BASEL PA VIADUKSTRASSE 40-44, PO BOX 133, CH-4010 BASEL, SWITZERLAND SN 0033-4553 J9 PURE APPL GEOPHYS JI Pure Appl. Geophys. PD APR PY 2008 VL 165 IS 3-4 BP 497 EP 521 DI 10.1007/s00024-008-0325-9 PG 25 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 301AA UT WOS:000255867100004 ER PT J AU Simpson, JR Landman, D Giroux, R Zeisset, M Hall, B Rhew, RD AF Simpson, James R. Landman, Drew Giroux, Rupert Zeisset, Michelle Hall, Brian Rhew, Ray D. TI Adapting second-order response surface designs to specific needs SO QUALITY AND RELIABILITY ENGINEERING INTERNATIONAL LA English DT Article DE response surface methodology; second-order designs; Box Behnken; prediction variance; Monte Carlo simulation; desirable design properties AB Experimental design strategies most often involve an initial choice of a classic factorial or response surface design and adapt that design to meet restrictions or unique requirements of the system under study. One such experience is described here, in which the objective was to develop an efficient experimental design strategy that would facilitate building second-order response models with excellent prediction capabilities. In development, careful consideration was paid to the desirable properties of response surface designs. Once developed, the proposed design was evaluated using Monte Carlo simulation to prove the concept, a pilot implementation of the design carried out to evaluate the accuracy of the response models, and a set of validation runs enacted to look for potential weaknesses in the approach. The purpose of the exercise was to develop a procedure to efficiently and effectively calibrate strain-gauge balances to be used in wind tunnel testing. The current calibration testing procedure is based on a time-intensive one-factor-at-a-time method. In this study, response surface methods were used to reduce the number of calibration runs required during the labor-intensive heavy load calibration, to leverage the prediction capabilities of response surface designs, and to provide an estimate of uncertainty for the calibration models. Results of the three-phased approach for design evaluation are presented. The new calibration process will require significantly fewer tests to achieve the same or improved levels of precision in balance calibration. Copyright (C) 2008 John Wiley & Sons, Ltd. C1 [Simpson, James R.; Giroux, Rupert; Zeisset, Michelle] Florida State Univ, Tallahassee, FL 32310 USA. [Landman, Drew] Old Dominion Univ, Norfolk, VA 23665 USA. [Hall, Brian; Rhew, Ray D.] NASA Langley, Hampton, VA 23605 USA. RP Simpson, JR (reprint author), Florida State Univ, Tallahassee, FL 32310 USA. NR 11 TC 8 Z9 8 U1 0 U2 1 PU JOHN WILEY & SONS LTD PI CHICHESTER PA THE ATRIUM, SOUTHERN GATE, CHICHESTER PO19 8SQ, W SUSSEX, ENGLAND SN 0748-8017 J9 QUAL RELIAB ENG INT JI Qual. Reliab. Eng. Int. PD APR PY 2008 VL 24 IS 3 BP 331 EP 349 DI 10.1002/qre.900 PG 19 WC Engineering, Multidisciplinary; Engineering, Industrial; Operations Research & Management Science SC Engineering; Operations Research & Management Science GA 292YY UT WOS:000255303200007 ER PT J AU Zeng, XP AF Zeng, Xiping TI The influence of radiation on ice crystal spectrum in the upper troposphere SO QUARTERLY JOURNAL OF THE ROYAL METEOROLOGICAL SOCIETY LA English DT Article DE cirrus; subvisual cloud; precipitation ID VAPOR-SPHERICAL MODEL; TERMINAL VELOCITIES; HYDROMETEOR GROWTH; CIRRUS CLOUDS; PARTICLES; WATER; CONDENSATION; ATMOSPHERES; CONVECTION; KINETICS AB This theoretical study is carried out to investigate the effect of radiation on ice crystal spectrum in the upper troposphere. First, an explicit expression is obtained for the ice crystal growth rate that takes account of radiative and kinetic effects. Second, the expression is used to quantitatively analyse how radiation broadens the ice crystal spectrum and then to reveal a new precipitation mechanism in the upper troposphere and the stratosphere. Third, the radiative effect is used to explain the subvisual clouds near the tropopause. Copyright (C) 2008 Royal Meteorological Society. C1 [Zeng, Xiping] NASA, Goddard Space Flight Ctr, Atmospheres Lab, Greenbelt, MD 20771 USA. [Zeng, Xiping] Univ Maryland Baltimore Cty, Goddard Earth Sci & Technol Ctr, Greenbelt, MD USA. RP Zeng, XP (reprint author), NASA, Goddard Space Flight Ctr, Atmospheres Lab, Mail Code 613-1, Greenbelt, MD 20771 USA. EM zeng@agnes.gsfc.nasa.gov NR 37 TC 3 Z9 3 U1 0 U2 2 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0035-9009 J9 Q J ROY METEOR SOC JI Q. J. R. Meteorol. Soc. PD APR PY 2008 VL 134 IS 632 BP 609 EP 620 DI 10.1002/qj.226 PN A PG 12 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 349PI UT WOS:000259292600005 ER PT J AU Foellmi, C Koenigsberger, G Georgiev, L Toledano, O Marchenko, SV Massey, P Dall, TH Moffat, AFJ Morrell, N Corcoran, M Kaufer, A Naze, Y Pittard, J St-Louis, N Fullerton, A Massa, D Pollock, AMT AF Foellmi, C. Koenigsberger, G. Georgiev, L. Toledano, O. Marchenko, S. V. Massey, P. Dall, T. H. Moffat, A. F. J. Morrell, N. Corcoran, M. Kaufer, A. Naze, Y. Pittard, J. St-Louis, N. Fullerton, A. Massa, D. Pollock, A. M. T. TI New insights into the nature of the SMC WR/LBV binary HD 5980 SO REVISTA MEXICANA DE ASTRONOMIA Y ASTROFISICA LA English DT Article DE binaries : close; stars : individual (HD 5980); stars : mass loss ID SMALL-MAGELLANIC-CLOUD; WOLF-RAYET BINARY; COLLIDING STELLAR WINDS; SYSTEM HD 5980; SPECTROSCOPIC MICROSCOPE; FUSE OBSERVATIONS; STAR HD-5980; V444 CYGNI; COMPONENTS; EMISSION AB We present the results of optical wavelength observations of the unusual SMC eclipsing binary system HD 5980 obtained in 1999 and 2004-2005. Radial velocity curves for the erupting LBV/WR object (star A) and its close WR-like companion (star B) are obtained by deblending the variable emission-line profiles of NIV and NV lines. The derived masses M-A = 58 - 79 M-circle dot and M-B = 51 - 67 M-circle dot, are more consistent with the the stars' location near the top of the HRD than previous estimates. The presence of a wind-wind interaction region is inferred from the orbital phase-dependent behavior of He I P Cygni absorption components. The emission-line intensities continued with the declining trend previously seen in UV spectra. The behavior of the photospheric absorption lines is consistent with the results of Schweickhardt (2000) who concludes that the third object in the combined spectrum, star C, is also a binary system with P-starC similar to 96.5 days, e=0.83. C1 [Foellmi, C.] Domaine Univ, Lab AstrOPhys Grenoble, F-38400 St Martin Dheres, France. [Corcoran, M.] NASA, Goddard Space Flight Ctr, CRESST, Greenbelt, MD 20771 USA. [Foellmi, C.] NASA, Goddard Space Flight Ctr, Xray Astrophys Lab, Greenbelt, MD 20771 USA. [Dall, T. H.] Gemini Obs, Hilo, HI 96720 USA. [Fullerton, A.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Georgiev, L.] Univ Nacl Autonoma Mexico, Inst Astron, Mexico City 04510, DF, Mexico. [Kaufer, A.] European So Observ, Santiago 19, Chile. [Koenigsberger, G.; Toledano, O.] Univ Nacl Autonoma Mexico, Inst Ciencias Fis, Cuernavaca 62210, Morelos, Mexico. [Marchenko, S. V.] Western Kentucky Univ, Dept Phys & Astron, Bowling Green, KY 42101 USA. [Massa, D.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Massey, P.] Lowell Observ, Flagstaff, AZ 86001 USA. [Moffat, A. F. J.] Univ Montreal, Dept Phys, Montreal, PQ H3C 3J7, Canada. [Morrell, N.] Carneige Obs, Las Campanas Obs, La Serena, Chile. [Naze, Y.] Univ Liege, Inst Astrophys & Gepphys, B-4000 Liege, Belgium. [Pittard, J.] Univ Leeds, Sch Phys & Astron, Leeds, W Yorkshire, England. [Pollock, A. M. T.] European Space Agcy, XMM Newton SOC, European Space Astron Ctr, Madrid 28691, Spain. RP Foellmi, C (reprint author), Domaine Univ, Lab AstrOPhys Grenoble, 414 Rue Piscine, F-38400 St Martin Dheres, France. EM cedric.foellmi@obs.ujf-grenoble.fr; gloria@fis.unam.mx; georgiev@dastroscu.unam.mx; toledano@hotmail.com; sergey@astro.wku.edu; Phil.Massey@lowell.edu; tdall@gemini.edu; moffat@astro.umontreal.ca; nidia@leoeps1.lco.cl; Michael.F.Corcoran.1@gsfc.nasa.gov; akaufer@eso.org; naze@astro.ulg.ac.be; jmp@ast.leeds.ac.uk; st-louis@astro.umontreal.ca; fullerton@4stsci.edu; massa@taotaomona.gsfc.nasa.gov; Andy.Pollock@sciops.esa.int OI Pittard, Julian/0000-0003-2244-5070; Naze, Yael/0000-0003-4071-9346 NR 43 TC 20 Z9 21 U1 2 U2 2 PU UNIV NACIONAL AUTONOMA MEXICO, INST DE ASTRONOMIA PI MEXICO CITY PA APDO POSTAL 70-264, MEXICO CITY 04510, MEXICO SN 0185-1101 J9 REV MEX ASTRON ASTR JI Rev. Mex. Astron. Astrofis. PD APR PY 2008 VL 44 IS 1 BP 3 EP 27 PG 25 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 285DY UT WOS:000254758700001 ER PT J AU Kiang, NY AF Kiang, Nancy Y. TI The color of plants on other worlds SO SCIENTIFIC AMERICAN LA English DT Article C1 NASA, Goddard Inst Space Studies, New York, NY 10025 USA. RP Kiang, NY (reprint author), NASA, Goddard Inst Space Studies, New York, NY 10025 USA. NR 0 TC 4 Z9 4 U1 3 U2 12 PU SCI AMERICAN INC PI NEW YORK PA 415 MADISON AVE, NEW YORK, NY 10017 USA SN 0036-8733 J9 SCI AM JI Sci.Am. PD APR PY 2008 VL 298 IS 4 BP 48 EP 55 PG 8 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 280RY UT WOS:000254445100028 PM 18380141 ER PT J AU Zhang, KQ Simard, M Ross, M Rivera-Monroy, VH Houle, P Ruiz, P Twilley, RR Whelan, KRT AF Zhang, Keqi Simard, Marc Ross, Michael Rivera-Monroy, Victor H. Houle, Patricia Ruiz, Pablo Twilley, Robert R. Whelan, Kevin R. T. TI Airborne laser scanning quantification of disturbances from hurricanes and lightning strikes to mangrove forests in Everglades National Park, USA SO SENSORS LA English DT Article DE airborne light detection and ranging (LIDAR); digital canopy model (DCM); forest disturbance; mangrove; hurricane; lightning strike; Everglades ID REGENERATION; VEGETATION; SEEDLINGS; SALINITY; BIOMASS; MODEL; LIDAR AB Airborne light detection and ranging ( LIDAR) measurements derived before and after Hurricanes Katrina and Wilma ( 2005) were used to quantify the impact of hurricanes and lightning strikes on the mangrove forest at two sites in Everglades National Park ( ENP). Analysis of LIDAR measurements covering 61 and 68 ha areas of mangrove forest at the Shark River and Broad River sites showed that the proportion of high tree canopy detected by the LIDAR after the 2005 hurricane season decreased significantly due to defoliation and breakage of branches and trunks, while the proportion of low canopy and the ground increased drastically. Tall mangrove forests distant from tidal creeks suffered more damage than lower mangrove forests adjacent to the tidal creeks. The hurricanes created numerous canopy gaps, and the number of gaps per square kilometer increased from about 400 similar to 500 to 4000 after Katrina and Wilma. The total area of gaps in the forest increased from about 1 similar to 2% of the total forest area to 12%. The relative contribution of hurricanes to mangrove forest disturbance in ENP is at least 2 times more than that from lightning strikes. However, hurricanes and lightning strikes disturb the mangrove forest in a related way. Most seedlings in lightning gaps survived the hurricane impact due to the protection of trees surrounding the gaps, and therefore provide an important resource for forest recovery after the hurricane. This research demonstrated that LIDAR is an effective remote sensing tool to quantify the effects of disturbances such as hurricanes and lightning strikes in the mangrove forest. C1 [Zhang, Keqi; Ross, Michael; Houle, Patricia; Ruiz, Pablo] Florida Int Univ, Dept Environm Studies, Miami, FL 33199 USA. [Zhang, Keqi; Houle, Patricia] Florida Int Univ, Int Hurricane Res Ctr, Miami, FL 33199 USA. [Simard, Marc] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Ross, Michael; Ruiz, Pablo] Florida Int Univ, SE Environm Res Ctr, Miami, FL 33199 USA. [Rivera-Monroy, Victor H.; Twilley, Robert R.] Louisiana State Univ, Wetland Biogeochem Inst, Dept Oceanog & Coastal Sci, Baton Rouge, LA 70803 USA. [Whelan, Kevin R. T.] Natl Pk Serv, S Florida & Caribbean Network, Inventory & Monitoring Program, Miami, FL 33157 USA. RP Zhang, KQ (reprint author), Florida Int Univ, Dept Environm Studies, Miami, FL 33199 USA. EM zhangk@fiu.edu RI Rivera-Monroy, Victor/G-7329-2011; Simard, Marc/H-3516-2013 OI Simard, Marc/0000-0002-9442-4562 NR 39 TC 24 Z9 26 U1 2 U2 11 PU MOLECULAR DIVERSITY PRESERVATION INT PI BASEL PA MATTHAEUSSTRASSE 11, CH-4057 BASEL, SWITZERLAND SN 1424-8220 J9 SENSORS-BASEL JI Sensors PD APR PY 2008 VL 8 IS 4 BP 2262 EP 2292 DI 10.3390/s8042262 PG 31 WC Chemistry, Analytical; Electrochemistry; Instruments & Instrumentation SC Chemistry; Electrochemistry; Instruments & Instrumentation GA 312AV UT WOS:000256642400012 PM 27879821 ER PT J AU Sun, CJ Wang, YQ Zhang, CJ Zhou, E Su, J AF Sun, Changjie Wang, Youqi Zhang, Congjian Zhou, Eric Su, Ji TI A modified self-consistent computational model for an electrostrictive graft elastomer SO SMART MATERIALS & STRUCTURES LA English DT Article ID FIELD AB An electrostrictive graft elastomer, as recently developed by NASA, is a type of electro-active polymer. In this paper, a 2D computational model with a self-consistent boundary is developed. Firstly, three-dimensional deformations, induced by both bending angle and dihedral torsional angle changes, are projected onto a two-dimensional plane. Using both theoretical and numerical analyses, the projected 2D equilibrium bending angle is shown to have the same value as the 3D equilibrium bending angle. The 2D equivalent bending stiffness is derived using a series model based upon the fact that both bending and dihedral torsion produce a configurational change. Equivalent stiffness is justified by polymer chain end-to-end distance characteristics. Secondly, a self-consistent scheme is developed to eliminate the boundary effect. Eight images of the unit cell are created peripherally, with the original unit cell in the center. Thus the boundary can only affect the rotation of the eight images, not the central unit cell. A computational model is employed to determine the electromechanical properties of the electrostrictive graft elastomer. Relations between electric field induced strain and electric field strength are calculated. The effect of molecular scale factors, such as free volume fraction, graft weight percentage and graft orientation, are also discussed. C1 [Sun, Changjie; Wang, Youqi; Zhang, Congjian; Zhou, Eric] Kansas State Univ, Dept Mech & Nucl Engn, Manhattan, KS 66506 USA. [Su, Ji] NASA, Langley Res Ctr, Hampton, VA 23681 USA. RP Wang, YQ (reprint author), Kansas State Univ, Dept Mech & Nucl Engn, Manhattan, KS 66506 USA. EM Wang@mne.ksu.edu NR 10 TC 4 Z9 4 U1 0 U2 6 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0964-1726 J9 SMART MATER STRUCT JI Smart Mater. Struct. PD APR PY 2008 VL 17 IS 2 AR 025007 DI 10.1088/0964-1726/17/2/025007 PG 8 WC Instruments & Instrumentation; Materials Science, Multidisciplinary SC Instruments & Instrumentation; Materials Science GA 276XF UT WOS:000254176300007 ER PT J AU Cadavid, AC Lawrence, JK Ruzmaikin, A AF Cadavid, A. C. Lawrence, J. K. Ruzmaikin, A. TI Principal components and independent component analysis of solar and space data SO SOLAR PHYSICS LA English DT Article; Proceedings Paper CT 3rd Solar Image Processing Workshop CY SEP, 2006 CL Trinity Coll, Dublin, ISRAEL HO Trinity Coll DE Methods : statistical; Sun : magnetic field ID MAGNETIC-FIELD FLUCTUATIONS; LONGITUDES; ROTATION; MODES; WIND AB Principal components analysis (PCA) and independent component analysis (ICA) are used to identify global patterns in solar and space data. PCA seeks orthogonal modes of the two-point correlation matrix constructed from a data set. It permits the identification of structures that remain coherent and correlated or that recur throughout a time series. ICA seeks for maximally independent modes and takes into account all order correlations of the data. We apply PCA to the interplanetary magnetic field polarity near 1 AU and to the 3.25R(circle dot) source-surface fields in the solar corona. The rotations of the two-sector structures of these systems vary together to high accuracy during the active interval of solar cycle 23. We then use PCA and ICA to hunt for preferred longitudes in northern hemisphere Carrington maps of magnetic fields. C1 [Cadavid, A. C.; Lawrence, J. K.] Calif State Univ Northridge, Dept Phys & Astron, Northridge, CA 91330 USA. [Ruzmaikin, A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Cadavid, AC (reprint author), Calif State Univ Northridge, Dept Phys & Astron, 18111 Nordhoff St, Northridge, CA 91330 USA. EM ana.cadavid@csun.edu NR 18 TC 12 Z9 12 U1 0 U2 3 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0038-0938 J9 SOL PHYS JI Sol. Phys. PD APR PY 2008 VL 248 IS 2 BP 247 EP 261 DI 10.1007/s11207-007-9026-2 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 290IE UT WOS:000255115700005 ER PT J AU Conlon, PA Gallagher, PT McAteer, RTJ Ireland, J Young, CA Kestener, P Hewett, RJ Maguire, K AF Conlon, P. A. Gallagher, P. T. McAteer, R. T. J. Ireland, J. Young, C. A. Kestener, P. Hewett, R. J. Maguire, K. TI Multifractal properties of evolving active regions SO SOLAR PHYSICS LA English DT Article; Proceedings Paper CT 3rd Solar Image Processing Workshop CY SEP, 2006 CL Trinity Coll, Dublin, ISRAEL HO Trinity Coll DE active regions; magnetic fields; turbulence ID SOLAR MAGNETIC-FIELDS; FLUX; MAGNETOGRAMS; MODEL AB Magnetohydrodynamic turbulence is thought to be responsible for producing complex, multiscale magnetic field distributions in solar active regions. Here we explore the multiscale properties of a number of evolving active regions using magnetograms from the Michelson Doppler Imager (MDI) on the Solar and Heliospheric Observatory (SOHO). The multifractal spectrum was obtained by using a modified box-counting method to study the relationship between magnetic-field multifractality and region evolution and activity. The initial emergence of each active region was found to be accompanied by characteristic changes in the multifractal spectrum. Specifically, the range of multifractal structures (D (div)) was found to increase during emergence, as was their significance or support (C (div)). Following this, a decrease in the range in multifractal structures occurred as the regions evolved to become large-scale, coherent structures. From the small sample considered, evidence was found for a direct relationship between the multifractal properties of the flaring regions and their flaring rate. C1 [Conlon, P. A.; Gallagher, P. T.] Trinity Coll Dublin, Astrophys Res Grp, Sch Phys, Dublin 2, Ireland. [McAteer, R. T. J.] Catholic Univ Amer, NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Ireland, J.; Young, C. A.] NASA, Goddard Space Flight Ctr, ADNET Syst Inc, Greenbelt, MD 20771 USA. [Kestener, P.] CEA Saclay, DSM, DAPNIA, SEDI, F-91191 Gif Sur Yvette, France. [Hewett, R. J.] Univ Illinois, Dept Comp Sci, Urbana, IL 61801 USA. [Maguire, K.] Univ Coll Dublin, Sch Phys, Dublin 4, Ireland. RP Conlon, PA (reprint author), Trinity Coll Dublin, Astrophys Res Grp, Sch Phys, Dublin 2, Ireland. EM conlon.paul@gmail.com RI McAteer, R. T. James/D-3736-2011; Gallagher, Peter/C-7717-2011 OI Gallagher, Peter/0000-0001-9745-0400 NR 26 TC 36 Z9 37 U1 1 U2 1 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0038-0938 J9 SOL PHYS JI Sol. Phys. PD APR PY 2008 VL 248 IS 2 BP 297 EP 309 DI 10.1007/s11207-007-9074-7 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 290IE UT WOS:000255115700008 ER PT J AU Jones, HP Chapman, GA Harvey, KL Pap, JM Preminger, DG Turmon, MJ Walton, SR AF Jones, H. P. Chapman, G. A. Harvey, K. L. Pap, J. M. Preminger, D. G. Turmon, M. J. Walton, S. R. TI A comparison of feature classification methods for modeling solar irradiance variation SO SOLAR PHYSICS LA English DT Article; Proceedings Paper CT 3rd Solar Image Processing Workshop CY SEP, 2006 CL Trinity Coll, Dublin, ISRAEL HO Trinity Coll DE solar irradiance; Sunspots; active regions; photosphere; data analysis ID SPECTRAL IRRADIANCE; CLIMATE-CHANGE; CYCLES 21-23; VARIABILITY; RECONSTRUCTION; SOLAR-CYCLE-23; LUMINOSITY; SUN AB Physical understanding of total and spectral solar irradiance variation depends upon establishing a connection between the temporal variability of spatially resolved solar structures and spacecraft observations of irradiance. One difficulty in comparing models derived from different data sets is that the many ways for identifying solar features such as faculae, sunspots, quiet Sun, and various types of "network" are not necessarily consistent. To learn more about classification differences and how they affect irradiance models, feature "masks" are compared as derived from five current methods: multidimensional histogram analysis of NASA/National Solar Observatory/Kitt Peak spectromagnetograph data, statistical pattern recognition applied to SOHO/Michelson Doppler Imager photograms and magnetograms, threshold masks allowing for influence of spatial surroundings applied to NSO magnetograms, and "one-trigger" and "three-trigger" algorithms applied to California State University at Northridge Cartesian Full Disk Telescope intensity observations. In general all of the methods point to the same areas of the Sun for labeling sunspots and active-region faculae, and available time series of area measurements from the methods correlate well with each other and with solar irradiance. However, some methods include larger label sets, and there are important differences in detail, with measurements of sunspot area differing by as much as a factor of two. The methods differ substantially regarding inclusion of fine spatial scale in the feature definitions. The implications of these differences for modeling solar irradiance variation are discussed. C1 [Jones, H. P.] Natl Solar Observ, Tucson, AZ 85726 USA. [Chapman, G. A.; Preminger, D. G.; Walton, S. R.] Calif State Univ Northridge, Dept Phys & Astron, Northridge, CA 91330 USA. [Harvey, K. L.] Solar Phys Res Corp, Tucson, AZ USA. [Pap, J. M.] NASA, Goddard Space Flight Ctr, UMBC, Goddard Earth Sci & Technol Inst, Greenbelt, MD 20771 USA. [Turmon, M. J.] CALTECH, NASA, Jet Prop Lab, Pasadena, CA 91125 USA. RP Jones, HP (reprint author), Natl Solar Observ, POB 26732, Tucson, AZ 85726 USA. EM hjones@nso.edu NR 31 TC 12 Z9 12 U1 0 U2 3 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0038-0938 J9 SOL PHYS JI Sol. Phys. PD APR PY 2008 VL 248 IS 2 BP 323 EP 337 DI 10.1007/s11207-007-9069-4 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 290IE UT WOS:000255115700010 ER PT J AU Young, CA Gallagher, PT AF Young, C. Alex Gallagher, Peter T. TI Multiscale edge detection in the corona SO SOLAR PHYSICS LA English DT Article; Proceedings Paper CT 3rd Solar Image Processing Workshop CY SEP, 2006 CL Trinity Coll, Dublin, ISRAEL HO Trinity Coll DE Sun : corona; Sun : coronal mass ejections (CMEs); techniques : image processing ID MASS EJECTIONS AB Coronal Mass Ejections (CMEs) are challenging objects to detect using automated techniques, due to their high velocity and diffuse, irregular morphology. A necessary step to automating the detection process is to first remove the subjectivity introduced by the observer used in the current, standard, CME detection and tracking method. Here we describe and demonstrate a multiscale edge detection technique that addresses this step and could serve as one part of an automated CME detection system. This method provides a way to objectively define a CME front with associated error estimates. These fronts can then be used to extract CME morphology and kinematics. We apply this technique to a CME observed on 18 April 2000 by the Large Angle Solar COronagraph experiment (LASCO) C2/C3 and a CME observed on 21 April 2002 by LASCO C2/C3 and the Transition Region and Coronal Explorer (TRACE). For the two examples in this work, the heights determined by the standard manual method are larger than those determined with the multiscale method by approximate to 10% using LASCO data and approximate to 20% using TRACE data. C1 [Young, C. Alex] NASA, Goddard Space Flight Ctr, ADNET Syst Inc, Greenbelt, MD 20771 USA. [Gallagher, Peter T.] Trinity Coll Dublin, Astrophys Res Grp, Sch Phys, Dublin 2, Ireland. RP Young, CA (reprint author), NASA, Goddard Space Flight Ctr, ADNET Syst Inc, Greenbelt, MD 20771 USA. EM c.alex.young@nasa.gov RI Gallagher, Peter/C-7717-2011 OI Gallagher, Peter/0000-0001-9745-0400 NR 19 TC 18 Z9 18 U1 1 U2 5 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0038-0938 J9 SOL PHYS JI Sol. Phys. PD APR PY 2008 VL 248 IS 2 BP 457 EP 469 DI 10.1007/s11207-008-9177-9 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 290IE UT WOS:000255115700018 ER PT J AU Kaiser, ML Kucera, TA Davila, JM Cyr, OCS Guhathakurta, M Christian, E AF Kaiser, M. L. Kucera, T. A. Davila, J. M. Cyr, O. C. St. Guhathakurta, M. Christian, E. TI The STEREO Mission: An introduction SO SPACE SCIENCE REVIEWS LA English DT Editorial Material DE CME; solar; three-dimensional AB The twin STEREO spacecraft were launched on October 26, 2006, at 00:52 UT from Kennedy Space Center aboard a Delta 7925 launch vehicle. After a series of highly eccentric Earth orbits with apogees beyond the moon, each spacecraft used close flybys of the moon to escape into orbits about the Sun near 1 AU. Once in heliospheric orbit, one spacecraft trails Earth while the other leads. As viewed from the Sun, the two spacecraft separate at approximately 44 to 45 degrees per year. The purposes of the STEREO Mission are to understand the causes and mechanisms of coronal mass ejection (CME) initiation and to follow the propagation of CMEs through the inner heliosphere to Earth. Researchers will use STEREO measurements to study the mechanisms and sites of energetic particle acceleration and to develop three-dimensional (3-D) time-dependent models of the magnetic topology, temperature, density and velocity of the solar wind between the Sun and Earth. To accomplish these goals, each STEREO spacecraft is equipped with an almost identical set of optical, radio and in situ particles and fields instruments provided by U.S. and European investigators. The SECCHI suite of instruments includes two white light coronagraphs, an extreme ultraviolet imager and two heliospheric white light imagers which track CMEs out to 1 AU. The IMPACT suite of instruments measures in situ solar wind electrons, energetic electrons, protons and heavier ions. IMPACT also includes a magnetometer to measure the in situ magnetic field strength and direction. The PLASTIC instrument measures the composition of heavy ions in the ambient plasma as well as protons and alpha particles. The S/WAVES instrument uses radio waves to track the location of CME-driven shocks and the 3-D topology of open field lines along which flow particles produced by solar flares. Each of the four instrument packages produce a small real-time stream of selected data for purposes of predicting space weather events at Earth. NOAA forecasters at the Space Environment Center and others will use these data in their space weather forecasting and their resultant products will be widely used throughout the world. In addition to the four instrument teams, there is substantial participation by modeling and theory oriented teams. All STEREO data are freely available through individual Web sites at the four Principal Investigator institutions as well as at the STEREO Science Center located at NASA Goddard Space Flight Center. C1 [Kaiser, M. L.; Kucera, T. A.; Davila, J. M.; Cyr, O. C. St.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Guhathakurta, M.; Christian, E.] NASA Headquarters, Washington, DC 20024 USA. RP Kaiser, ML (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. EM Michael.Kaiser@nasa.gov RI Kucera, Therese/C-9558-2012; Christian, Eric/D-4974-2012; OI Christian, Eric/0000-0003-2134-3937; Kucera, Therese/0000-0001-9632-447X NR 18 TC 553 Z9 568 U1 8 U2 46 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0038-6308 J9 SPACE SCI REV JI Space Sci. Rev. PD APR PY 2008 VL 136 IS 1-4 BP 5 EP 16 DI 10.1007/s11214-007-9277-0 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 322OC UT WOS:000257384200002 ER PT J AU Biesecker, DA Webb, DF Cyr, OCS AF Biesecker, D. A. Webb, D. F. Cyr, O. C. St. TI STEREO space weather and the Space Weather Beacon SO SPACE SCIENCE REVIEWS LA English DT Review DE STEREO; space weather; coronal mass ejection; solar wind; forecasting ID CORONAL MASS EJECTIONS; ADVANCED COMPOSITION EXPLORER; JANUARY 1997; MAGNETIC CLOUD; EARTH; TIME; ELECTRON; STORMS AB The Solar Terrestrial Relations Observatory (STEREO) is primarily a solar and interplanetary research mission, with one of the natural applications being in the area of space weather. The obvious potential for space weather applications is so great that NOAA has worked to incorporate the real-time data into their forecast center as much as possible. A subset of the STEREO data will be continuously downlinked in a real-time broadcast mode, called the Space Weather Beacon. Within the research community there has been considerable interest in conducting space weather related research with STEREO. Some of this research is geared towards making an immediate impact while other work is still very much in the research domain. There are many areas where STEREO might contribute and we cannot predict where all the successes will come. Here we discuss how STEREO will contribute to space weather and many of the specific research projects proposed to address STEREO space weather issues. The data which will be telemetered down in the Space Weather Beacon is also summarized here. Some of the lessons learned from integrating other NASA missions into the forecast center are presented. We also discuss some specific uses of the STEREO data in the NOAA Space Environment Center. C1 [Biesecker, D. A.] NOAA, Space Environm Ctr, Boulder, CO 80305 USA. [Webb, D. F.] Boston Coll, Inst Sci Res, Chestnut Hill, MA 02467 USA. [Cyr, O. C. St.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Biesecker, DA (reprint author), NOAA, Space Environm Ctr, 325 Broadway, Boulder, CO 80305 USA. EM doug.biesecker@noaa.gov NR 54 TC 10 Z9 10 U1 0 U2 3 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0038-6308 EI 1572-9672 J9 SPACE SCI REV JI Space Sci. Rev. PD APR PY 2008 VL 136 IS 1-4 BP 45 EP 65 DI 10.1007/s11214-007-9165-7 PG 21 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 322OC UT WOS:000257384200004 ER PT J AU Howard, RA Moses, JD Vourlidas, A Newmark, JS Socker, DG Plunkett, SP Korendyke, CM Cook, JW Hurley, A Davila, JM Thompson, WT St Cyr, OC Mentzell, E Mehalick, K Lemen, JR Wuelser, JP Duncan, DW Tarbell, TD Wolfson, CJ Moore, A Harrison, RA Waltham, NR Lang, J Davis, CJ Eyles, CJ Mapson-Menard, H Simnett, GM Halain, JP Defise, JM Mazy, E Rochus, P Mercier, R Ravet, MF Delmotte, F Auchere, F Delaboudiniere, JP Bothmer, V Deutsch, W Wang, D Rich, N Cooper, S Stephens, V Maahs, G Baugh, R McMullin, D Carter, T AF Howard, R. A. Moses, J. D. Vourlidas, A. Newmark, J. S. Socker, D. G. Plunkett, S. P. Korendyke, C. M. Cook, J. W. Hurley, A. Davila, J. M. Thompson, W. T. St Cyr, O. C. Mentzell, E. Mehalick, K. Lemen, J. R. Wuelser, J. P. Duncan, D. W. Tarbell, T. D. Wolfson, C. J. Moore, A. Harrison, R. A. Waltham, N. R. Lang, J. Davis, C. J. Eyles, C. J. Mapson-Menard, H. Simnett, G. M. Halain, J. P. Defise, J. M. Mazy, E. Rochus, P. Mercier, R. Ravet, M. F. Delmotte, F. Auchere, F. Delaboudiniere, J. P. Bothmer, V. Deutsch, W. Wang, D. Rich, N. Cooper, S. Stephens, V. Maahs, G. Baugh, R. McMullin, D. Carter, T. TI Sun Earth Connection Coronal and Heliospheric Investigation (SECCHI) SO SPACE SCIENCE REVIEWS LA English DT Review DE solar corona; Lyot coronagraph; XUV heliograph; heliospheric imager; coronal loops; coronal mass ejections; stereo; heliosphere ID TRANSITION REGION; ATOMIC DATABASE; EMISSION-LINES; IMAGER; EXPLORER; CHIANTI AB The Sun Earth Connection Coronal and Heliospheric Investigation (SECCHI) is a five telescope package, which has been developed for the Solar Terrestrial Relation Observatory (STEREO) mission by the Naval Research Laboratory (USA), the Lockheed Solar and Astrophysics Laboratory (USA), the Goddard Space Flight Center (USA), the University of Birmingham (UK), the Rutherford Appleton Laboratory (UK), the Max Planck Institute for Solar System Research (Germany), the Centre Spatiale de Leige (Belgium), the Institut d'Optique (France) and the Institut d'Astrophysique Spatiale (France). SECCHI comprises five telescopes, which together image the solar corona from the solar disk to beyond 1 AU. These telescopes are: an extreme ultraviolet imager (EUVI: 1-1.7 R-circle dot), two traditional Lyot coronagraphs (COR1: 1.5-4 R-circle dot and COR2: 2.5-15 R-circle dot) and two new designs of heliospheric imagers (HI-1: 15-84 R-circle dot and HI-2: 66-318 R-circle dot). All the instruments use 2048x2048 pixel CCD arrays in a backside-in mode. The EUVI backside surface has been specially processed for EUV sensitivity, while the others have an anti-reflection coating applied. A multi-tasking operating system, running on a PowerPC CPU, receives commands from the spacecraft, controls the instrument operations, acquires the images and compresses them for downlink through the main science channel (at compression factors typically up to 20x) and also through a low bandwidth channel to be used for space weather forecasting (at compression factors up to 200x). An image compression factor of about 10x enable the collection of images at the rate of about one every 2-3 minutes. Identical instruments, except for different sizes of occulters, are included on the STEREO-A and STEREO-B spacecraft. C1 [Howard, R. A.; Moses, J. D.; Vourlidas, A.; Newmark, J. S.; Socker, D. G.; Plunkett, S. P.; Korendyke, C. M.; Cook, J. W.; Hurley, A.] USN, Res Lab, EO Hulburt Ctr Space Res, Washington, DC 20375 USA. [Davila, J. M.; Thompson, W. T.; St Cyr, O. C.; Mentzell, E.; Mehalick, K.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20742 USA. [Lemen, J. R.; Wuelser, J. P.; Duncan, D. W.; Tarbell, T. D.; Wolfson, C. J.; Moore, A.] Lockheed Martin Solar & Astrophys Lab, Palo Alto, CA 94304 USA. [Harrison, R. A.; Waltham, N. R.; Lang, J.; Davis, C. J.] Rutherford Appleton Lab, Space Sci & Technol Dept, Didcot OX11 OQX, Oxon, England. [Eyles, C. J.; Mapson-Menard, H.; Simnett, G. M.] Univ Birmingham, Astrophys & Space Res Grp, Birmingham B15 2TT, W Midlands, England. [Halain, J. P.; Defise, J. M.; Mazy, E.; Rochus, P.] Univ Liege, Ctr Spatiale Liege, B-4031 Angleur, Belgium. [Auchere, F.; Delaboudiniere, J. P.] Ctr Univ Orsay, Inst Astrophys Spatiale, F-91405 Orsay, France. [Bothmer, V.] Univ Gottingen, Inst Astrophys, Max Planck Inst Solar Syst Res, D-37077 Gottingen, Germany. [Deutsch, W.] Max Planck Inst Solar Syst Res, Katlenburg Lindau, Germany. [Wang, D.; Rich, N.] Interferometr Inc, Herndon, VA USA. [Cooper, S.; Stephens, V.; Maahs, G.] HYTEC Inc, Los Alamos, NM 87544 USA. [Baugh, R.; McMullin, D.; Carter, T.] Praxis Inc, Alexandria, VA 22303 USA. RP Howard, RA (reprint author), USN, Res Lab, EO Hulburt Ctr Space Res, Washington, DC 20375 USA. EM russ.howard@nrl.navy.mil RI Vourlidas, Angelos/C-8231-2009; Thompson, William/D-7376-2012; Scott, Christopher/H-8664-2012; OI Vourlidas, Angelos/0000-0002-8164-5948; Scott, Christopher/0000-0001-6411-5649; Auchere, Frederic/0000-0003-0972-7022 NR 25 TC 762 Z9 775 U1 8 U2 41 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0038-6308 EI 1572-9672 J9 SPACE SCI REV JI Space Sci. Rev. PD APR PY 2008 VL 136 IS 1-4 BP 67 EP 115 DI 10.1007/s11214-008-9341-4 PG 49 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 322OC UT WOS:000257384200005 ER PT J AU Luhmann, JG Curtis, DW Schroeder, P McCauley, J Lin, RP Larson, DE Bale, SD Sauvaud, JA Aoustin, C Mewaldt, RA Cummings, AC Stone, EC Davis, AJ Cook, WR Kecman, B Wiedenbeck, ME von Rosenvinge, T Acuna, MH Reichenthal, LS Shuman, S Wortman, KA Reames, DV Mueller-Mellin, R Kunow, H Mason, GM Walpole, P Korth, A Sanderson, TR Russell, CT Gosling, JT AF Luhmann, J. G. Curtis, D. W. Schroeder, P. McCauley, J. Lin, R. P. Larson, D. E. Bale, S. D. Sauvaud, J. -A. Aoustin, C. Mewaldt, R. A. Cummings, A. C. Stone, E. C. Davis, A. J. Cook, W. R. Kecman, B. Wiedenbeck, M. E. von Rosenvinge, T. Acuna, M. H. Reichenthal, L. S. Shuman, S. Wortman, K. A. Reames, D. V. Mueller-Mellin, R. Kunow, H. Mason, G. M. Walpole, P. Korth, A. Sanderson, T. R. Russell, C. T. Gosling, J. T. TI STEREO IMPACT investigation goals, measurements, and data products overview SO SPACE SCIENCE REVIEWS LA English DT Review DE STEREO; coronal mass ejection; solar energetic particles; suprathermal electrons; solar wind electrons; interplanetary magnetic field; multipoint heliospheric measurements ID CORONAL MASS EJECTIONS; SOLAR ENERGETIC PARTICLES; INTERPLANETARY MAGNETIC-FIELD; COROTATING INTERACTION REGIONS; HYDROMAGNETIC WAVE EXCITATION; ADVANCED COMPOSITION EXPLORER; INTER-PLANETARY SHOCK; HEAT-FLUX DROPOUTS; 1 AU; 3-DIMENSIONAL PROPAGATION AB The IMPACT (In situ Measurements of Particles And CME Transients) investigation on the STEREO mission was designed and developed to provide multipoint solar wind and suprathermal electron, interplanetary magnetic field, and solar energetic particle information required to unravel the nature of coronal mass ejections and their heliospheric consequences. IMPACT consists of seven individual sensors which are packaged into a boom suite, and a SEP suite. This review summarizes the science objectives of IMPACT, the instruments that comprise the IMPACT investigation, the accommodation of IMPACT on the STEREO twin spacecraft, and the overall data products that will flow from the IMPACT measurements. Accompanying papers in this volume of Space Science Reviews highlight the individual sensor technical details and capabilities, STEREO project plans for the use of IMPACT data, and modeling activities for IMPACT (and other STEREO) data interpretation. C1 [Luhmann, J. G.; Curtis, D. W.; Schroeder, P.; McCauley, J.; Lin, R. P.; Larson, D. E.; Bale, S. D.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Sauvaud, J. -A.; Aoustin, C.] CESR, F-31028 Toulouse 4, France. [Mewaldt, R. A.; Cummings, A. C.; Stone, E. C.; Davis, A. J.; Cook, W. R.; Kecman, B.] CALTECH, Pasadena, CA 91125 USA. [Wiedenbeck, M. E.] Jet Prop Lab, Pasadena, CA 91109 USA. [von Rosenvinge, T.; Acuna, M. H.; Reichenthal, L. S.; Shuman, S.; Wortman, K. A.; Reames, D. V.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Mueller-Mellin, R.; Kunow, H.; Mason, G. M.] Univ Kiel, D-24118 Kiel, Germany. [Mason, G. M.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA. [Walpole, P.] Univ Maryland, College Pk, MD 20742 USA. [Korth, A.] Max Planck Inst Sonnensyst Forsch, Lindau, Germany. [Sanderson, T. R.] ESA, Res & Sci Support Div, Noordwijk, Netherlands. [Russell, C. T.] Univ Calif Los Angeles, Inst Geophys & Planetary Phys, Los Angeles, CA 90095 USA. [Gosling, J. T.] Univ Colorado, Atmospher & Space Phys Lab, Boulder, CO 80309 USA. RP Luhmann, JG (reprint author), Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. EM jgluhman@ss1.berkeley.edu RI Bale, Stuart/E-7533-2011 OI Bale, Stuart/0000-0002-1989-3596 NR 167 TC 136 Z9 137 U1 2 U2 9 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0038-6308 J9 SPACE SCI REV JI Space Sci. Rev. PD APR PY 2008 VL 136 IS 1-4 BP 117 EP 184 DI 10.1007/s11214-007-9170-x PG 68 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 322OC UT WOS:000257384200006 ER PT J AU Acuna, MH Curtis, D Scheifele, JL Russell, CT Schroeder, P Szabo, A Luhmann, JG AF Acuna, M. H. Curtis, D. Scheifele, J. L. Russell, C. T. Schroeder, P. Szabo, A. Luhmann, J. G. TI The STEREO/IMPACT magnetic field experiment SO SPACE SCIENCE REVIEWS LA English DT Review DE STEREO mission; IMPACT; space weather; interplanetary medium; solar physics ID HYDROMAGNETIC WAVE EXCITATION; INTERPLANETARY TRAVELING SHOCKS; RANKINE-HUGONIOT PROBLEM; SOLAR-WIND; ION-ACCELERATION; BOW SHOCK; MAGNETOMETERS; TURBULENCE; EVOLUTION; UPSTREAM AB The magnetometer on the STEREO mission is one of the sensors in the IMPACT instrument suite. A single, triaxial, wide-range, low-power and noise fluxgate magnetometer of traditional design-and reduced volume configuration-has been implemented in each spacecraft. The sensors are mounted on the IMPACT telescoping booms at a distance of similar to 3 m from the spacecraft body to reduce magnetic contamination. The electronics have been designed as an integral part of the IMPACT Data Processing Unit, sharing a common power converter and data/command interfaces. The instruments cover the range +/- 65,536 nT in two intervals controlled by the IDPU (+/- 512 nT; +/- 65,536 nT). This very wide range allows operation of the instruments during all phases of the mission, including Earth flybys as well as during spacecraft test and integration in the geomagnetic field. The primary STEREO/IMPACT science objectives addressed by the magnetometer are the study of the interplanetary magnetic field (IMF), its response to solar activity, and its relationship to solar wind structure. The instruments were powered on and the booms deployed on November 1, 2006, seven days after the spacecraft were launched, and are operating nominally. A magnetic cleanliness program was implemented to minimize variable spacecraft fields and to ensure that the static spacecraft-generated magnetic field does not interfere with the measurements. C1 [Acuna, M. H.; Scheifele, J. L.; Szabo, A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Curtis, D.; Schroeder, P.; Luhmann, J. G.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Russell, C. T.] Univ Calif Los Angeles, Inst Geophys & Planetary Phys, Los Angeles, CA 90024 USA. RP Acuna, MH (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. EM mario.acuna@nasa.gov NR 45 TC 124 Z9 124 U1 0 U2 12 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0038-6308 J9 SPACE SCI REV JI Space Sci. Rev. PD APR PY 2008 VL 136 IS 1-4 BP 203 EP 226 DI 10.1007/s11214-007-9259-2 PG 24 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 322OC UT WOS:000257384200008 ER PT J AU Mason, GM Korth, A Walpole, PH Desai, MI Von Rosenvinge, TT Shuman, SA AF Mason, G. M. Korth, A. Walpole, P. H. Desai, M. I. Von Rosenvinge, T. T. Shuman, S. A. TI The Suprathermal Ion Telescope (SIT) for the IMPACT/SEP investigation SO SPACE SCIENCE REVIEWS LA English DT Review DE solar energetic particles (SEPs); cosmic rays; shock acceleration; CMEs ID ENERGETIC PARTICLE EVENTS; HE-3-RICH SOLAR-FLARES; COROTATING INTERACTION REGIONS; INTERPLANETARY SHOCKS; HEAVY-IONS; 1 AU; SPECTRAL PROPERTIES; SEED POPULATION; HIGH-ENERGIES; ACCELERATION AB The Solar-Terrestrial Relations Observatory (STEREO) mission addresses critical problems of the physics of explosive disturbances in the solar corona, and their propagation and interactions in the interplanetary medium between the Sun and Earth. The In-Situ-Measurements of Particles and CME Transients (IMPACT) investigation observes the consequences of these disturbances and other transients at 1 AU. The generation of energetic particles is a fundamentally important feature of shock-associated Coronal Mass Ejections (CMEs) and other transients in the interplanetary medium. Multiple sensors within the IMPACT suite measure the particle population from energies just above the solar wind up to hundreds of MeV/nucleon. This paper describes a portion of the IMPACT Solar Energetic Particles (SEP) package, the Suprathermal Ion Telescope (SIT) which identifies the heavy ion composition from the suprathermal through the energetic particle range (similar to few 10 s of keV/nucleon to several MeV/nucleon). SIT will trace and identify processes that energize low energy ions, and characterize their transport in the interplanetary medium. SIT is a time-of-flight mass spectrometer with high sensitivity designed to derive detailed multi-species particle spectra with a cadence of 60 s, thereby enabling detailed studies of shock-accelerated and other energetic particle populations observed at 1 AU. C1 [Mason, G. M.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA. [Korth, A.] Max Planck Inst Sonnesyst Forsch, Lindau, Germany. [Walpole, P. H.] Univ Maryland, College Pk, MD 20742 USA. [Desai, M. I.] SW Res Inst, San Antonio, TX 78238 USA. [Von Rosenvinge, T. T.; Shuman, S. A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Mason, GM (reprint author), Johns Hopkins Univ, Appl Phys Lab, Johns Hopkins Rd, Laurel, MD 20723 USA. EM glenn.mason@jhup1.edu NR 49 TC 36 Z9 36 U1 0 U2 0 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0038-6308 EI 1572-9672 J9 SPACE SCI REV JI Space Sci. Rev. PD APR PY 2008 VL 136 IS 1-4 BP 257 EP 284 DI 10.1007/s11214-006-9087-9 PG 28 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 322OC UT WOS:000257384200011 ER PT J AU Mewaldt, RA Cohen, CMS Cook, WR Cummings, AC Davis, AJ Geier, S Kecman, B Klemic, J Labrador, AW Leske, RA Miyasaka, H Nguyen, V Ogliore, RC Stone, EC Radocinski, RG Wiedenbeck, ME Hawk, J Shuman, S von Rosenvinge, TT Wortman, K AF Mewaldt, R. A. Cohen, C. M. S. Cook, W. R. Cummings, A. C. Davis, A. J. Geier, S. Kecman, B. Klemic, J. Labrador, A. W. Leske, R. A. Miyasaka, H. Nguyen, V. Ogliore, R. C. Stone, E. C. Radocinski, R. G. Wiedenbeck, M. E. Hawk, J. Shuman, S. von Rosenvinge, T. T. Wortman, K. TI The Low-Energy Telescope (LET) and SEP Central electronics for the STEREO mission SO SPACE SCIENCE REVIEWS LA English DT Review DE space vehicles : instruments; instrumentation : detectors; Sun : particle emission; Sun : coronal mass ejections; Sun : flares; acceleration of particles ID COROTATING INTERACTION REGIONS; SOLAR PARTICLE EVENTS; ADVANCED COMPOSITION EXPLORER; RAY ISOTOPE SPECTROMETER; CHARGE STATES; COSMIC-RAYS; TERMINATION SHOCK; HE-3-RICH EVENTS; NEURAL-NETWORKS; MAGNETIC-FIELD AB The Low-Energy Telescope (LET) is one of four sensors that make up the Solar Energetic Particle (SEP) instrument of the IMPACT investigation for NASA's STEREO mission. The LET is designed to measure the elemental composition, energy spectra, angular distributions, and arrival times of H to Ni ions over the energy range from similar to 3 to similar to 30 MeV/nucleon. It will also identify the rare isotope (3)He and trans-iron nuclei with 30 <= Z <= 83. The SEP measurements from the two STEREO spacecraft will be combined with data from ACE and other 1-AU spacecraft to provide multipoint investigations of the energetic particles that result from interplanetary shocks driven by coronal mass ejections (CMEs) and from solar flare events. The multipoint in situ observations of SEPs and solar-wind plasma will complement STEREO images of CMEs in order to investigate their role in space weather. Each LET instrument includes a sensor system made up of an array of 14 solid-state detectors composed of 54 segments that are individually analyzed by custom Pulse Height Analysis System Integrated Circuits (PHASICs). The signals from four PHASIC chips in each LET are used by a Minimal Instruction Set Computer (MISC) to provide onboard particle identification of a dozen species in similar to 12 energy intervals at event rates of similar to 1,000 events/sec. An additional control unit, called SEP Central, gathers data from the four SEP sensors, controls the SEP bias supply, and manages the interfaces to the sensors and the SEP interface to the Instrument Data Processing Unit (IDPU). This article outlines the scientific objectives that LET will address, describes the design and operation of LET and the SEP Central electronics, and discusses the data products that will result. C1 [Mewaldt, R. A.; Cohen, C. M. S.; Cook, W. R.; Cummings, A. C.; Davis, A. J.; Geier, S.; Kecman, B.; Klemic, J.; Labrador, A. W.; Leske, R. A.; Miyasaka, H.; Nguyen, V.; Ogliore, R. C.; Stone, E. C.] CALTECH, Pasadena, CA 91125 USA. [Radocinski, R. G.; Wiedenbeck, M. E.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Hawk, J.; Shuman, S.; von Rosenvinge, T. T.; Wortman, K.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Mewaldt, RA (reprint author), CALTECH, Pasadena, CA 91125 USA. EM rmewaldt@sr1.caltech.edu NR 101 TC 57 Z9 58 U1 0 U2 3 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0038-6308 J9 SPACE SCI REV JI Space Sci. Rev. PD APR PY 2008 VL 136 IS 1-4 BP 285 EP 362 DI 10.1007/s11214-007-9288-x PG 78 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 322OC UT WOS:000257384200012 ER PT J AU von Rosenvinge, TT Reames, DV Baker, R Hawk, J Nolan, JT Ryan, L Shuman, S Wortman, KA Mewaldt, RA Cummings, AC Cook, WR Labrador, AW Leske, RA Wiedenbeck, ME AF von Rosenvinge, T. T. Reames, D. V. Baker, R. Hawk, J. Nolan, J. T. Ryan, L. Shuman, S. Wortman, K. A. Mewaldt, R. A. Cummings, A. C. Cook, W. R. Labrador, A. W. Leske, R. A. Wiedenbeck, M. E. TI The High Energy Telescope for STEREO SO SPACE SCIENCE REVIEWS LA English DT Review DE space instrumentation; STEREO mission; energetic particles; coronal mass ejections; particle acceleration ID STORM PARTICLES; SOLAR; EXPLORER; EVENTS AB The IMPACT investigation for the STEREO Mission includes a complement of Solar Energetic Particle instruments on each of the two STEREO spacecraft. Of these instruments, the High Energy Telescopes (HETs) provide the highest energy measurements. This paper describes the HETs in detail, including the scientific objectives, the sensors, the overall mechanical and electrical design, and the on-board software. The HETs are designed to measure the abundances and energy spectra of electrons, protons, He, and heavier nuclei up to Fe in interplanetary space. For protons and He that stop in the HET, the kinetic energy range corresponds to similar to 13 to 40 MeV/n. Protons that do not stop in the telescope (referred to as penetrating protons) are measured up to similar to 100 MeV/n, as are penetrating He. For stopping He, the individual isotopes (3)He and (4)He can be distinguished. Stopping electrons are measured in the energy range similar to 0.7-6 MeV. C1 [von Rosenvinge, T. T.; Reames, D. V.; Baker, R.; Hawk, J.; Nolan, J. T.; Ryan, L.; Shuman, S.; Wortman, K. A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Mewaldt, R. A.; Cummings, A. C.; Cook, W. R.; Labrador, A. W.; Leske, R. A.] CALTECH, Pasadena, CA 91125 USA. [Wiedenbeck, M. E.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP von Rosenvinge, TT (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. EM Tycho.T.vonRosenvinge@nasa.gov NR 18 TC 40 Z9 40 U1 0 U2 2 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0038-6308 J9 SPACE SCI REV JI Space Sci. Rev. PD APR PY 2008 VL 136 IS 1-4 BP 391 EP 435 DI 10.1007/s11214-007-9300-5 PG 45 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 322OC UT WOS:000257384200014 ER PT J AU Galvin, AB Kistler, LM Popecki, MA Farrugia, CJ Simunac, KDC Ellis, L Mobius, E Lee, MA Boehm, M Carroll, J Crawshaw, A Conti, M Demaine, P Ellis, S Gaidos, JA Googins, J Granoff, M Gustafson, A Heirtzler, D King, B Knauss, U Levasseur, J Longworth, S Singer, K Turco, S Vachon, P Vosbury, M Widholm, M Blush, LM Karrer, R Bochsler, P Daoudi, H Etter, A Fischer, J Jost, J Opitz, A Sigrist, M Wurz, P Klecker, B Ertl, M Seidenschwang, E Wimmer-Schweingruber, RF Koeten, M Thompson, B Steinfeld, D AF Galvin, A. B. Kistler, L. M. Popecki, M. A. Farrugia, C. J. Simunac, K. D. C. Ellis, L. Moebius, E. Lee, M. A. Boehm, M. Carroll, J. Crawshaw, A. Conti, M. Demaine, P. Ellis, S. Gaidos, J. A. Googins, J. Granoff, M. Gustafson, A. Heirtzler, D. King, B. Knauss, U. Levasseur, J. Longworth, S. Singer, K. Turco, S. Vachon, P. Vosbury, M. Widholm, M. Blush, L. M. Karrer, R. Bochsler, P. Daoudi, H. Etter, A. Fischer, J. Jost, J. Opitz, A. Sigrist, M. Wurz, P. Klecker, B. Ertl, M. Seidenschwang, E. Wimmer-Schweingruber, R. F. Koeten, M. Thompson, B. Steinfeld, D. TI The Plasma and Suprathermal Ion Composition (PLASTIC) investigation on the STEREO observatories SO SPACE SCIENCE REVIEWS LA English DT Review DE STEREO; solar wind; plasma; suprathermal; composition; time-of-flight spectrometer; coronal mass ejections; multipoint spacecraft observations ID COROTATING INTERACTION REGIONS; SOLAR ENERGETIC PARTICLE; CORONAL MASS EJECTIONS; WIND STREAM INTERFACES; THIN CARBON FOILS; CHARGE STATES; ELECTRON-EMISSION; PICKUP IONS; INTERPLANETARY SHOCKS; CALIBRATION SYSTEM AB The Plasma and Suprathermal Ion Composition (PLASTIC) investigation provides the in situ solar wind and low energy heliospheric ion measurements for the NASA Solar Terrestrial Relations Observatory Mission, which consists of two spacecraft (STEREO-A, STEREO-B). PLASTIC-A and PLASTIC-B are identical. Each PLASTIC is a time-of-flight/energy mass spectrometer designed to determine the elemental composition, ionic charge states, and bulk flow parameters of major solar wind ions in the mass range from hydrogen to iron. PLASTIC has nearly complete angular coverage in the ecliptic plane and an energy range from similar to 0.3 to 80 keV/e, from which the distribution functions of suprathermal ions, including those ions created in pick-up and local shock acceleration processes, are also provided. C1 [Galvin, A. B.; Kistler, L. M.; Popecki, M. A.; Farrugia, C. J.; Simunac, K. D. C.; Ellis, L.; Moebius, E.; Lee, M. A.; Boehm, M.; Carroll, J.; Crawshaw, A.; Conti, M.; Demaine, P.; Ellis, S.; Gaidos, J. A.; Googins, J.; Granoff, M.; Gustafson, A.; Heirtzler, D.; King, B.; Knauss, U.; Levasseur, J.; Longworth, S.; Singer, K.; Turco, S.; Vachon, P.; Vosbury, M.; Widholm, M.] Univ New Hampshire, Inst Study Earth Oceans & Space, Durham, NH 03824 USA. [Galvin, A. B.; Kistler, L. M.; Farrugia, C. J.; Simunac, K. D. C.; Moebius, E.; Lee, M. A.] Univ New Hampshire, Dept Phys, Durham, NH 03824 USA. [Blush, L. M.; Karrer, R.; Bochsler, P.; Daoudi, H.; Etter, A.; Fischer, J.; Jost, J.; Opitz, A.; Sigrist, M.; Wurz, P.] Univ Bern, Inst Phys, CH-3012 Bern, Switzerland. [Klecker, B.; Ertl, M.; Seidenschwang, E.] Max Planck Inst Extraterr Phys, D-85741 Garching, Germany. [Wimmer-Schweingruber, R. F.; Koeten, M.] Univ Kiel, Inst Expt & Appl Phys, Extraterr Phys, D-24098 Kiel, Germany. [Thompson, B.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Steinfeld, D.] Orbital Sci Corp, Greenbelt, MD 20770 USA. RP Galvin, AB (reprint author), Univ New Hampshire, Inst Study Earth Oceans & Space, SSC Morse Hall, Durham, NH 03824 USA. EM toni.galvin@unh.edu RI Galvin, Antoinette/A-6114-2013; Thompson, Barbara/C-9429-2012; OI Moebius, Eberhard/0000-0002-2745-6978 NR 103 TC 217 Z9 219 U1 2 U2 14 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0038-6308 J9 SPACE SCI REV JI Space Sci. Rev. PD APR PY 2008 VL 136 IS 1-4 BP 437 EP 486 DI 10.1007/s11214-007-9296-x PG 50 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 322OC UT WOS:000257384200015 ER PT J AU Bougeret, JL Goetz, K Kaiser, ML Bale, SD Kellogg, PJ Maksimovic, M Monge, N Monson, SJ Astier, PL Davy, S Dekkali, M Hinze, JJ Manning, RE Aguilar-Rodriguez, E Bonnin, X Briand, C Cairns, IH Cattell, CA Cecconi, B Eastwood, J Ergun, RE Fainberg, J Hoang, S Huttunen, KEJ Krucker, S Lecacheux, A MacDowall, RJ Macher, W Mangeney, A Meetre, CA Moussas, X Nguyen, QN Oswald, TH Pulupa, M Reiner, MJ Robinson, PA Rucker, H Salem, C Santolik, O Silvis, JM Ullrich, R Zarka, P Zouganelis, I AF Bougeret, J. L. Goetz, K. Kaiser, M. L. Bale, S. D. Kellogg, P. J. Maksimovic, M. Monge, N. Monson, S. J. Astier, P. L. Davy, S. Dekkali, M. Hinze, J. J. Manning, R. E. Aguilar-Rodriguez, E. Bonnin, X. Briand, C. Cairns, I. H. Cattell, C. A. Cecconi, B. Eastwood, J. Ergun, R. E. Fainberg, J. Hoang, S. Huttunen, K. E. J. Krucker, S. Lecacheux, A. MacDowall, R. J. Macher, W. Mangeney, A. Meetre, C. A. Moussas, X. Nguyen, Q. N. Oswald, T. H. Pulupa, M. Reiner, M. J. Robinson, P. A. Rucker, H. Salem, C. Santolik, O. Silvis, J. M. Ullrich, R. Zarka, P. Zouganelis, I. TI S/WAVES: The radio and plasma wave investigation on the STEREO Mission SO SPACE SCIENCE REVIEWS LA English DT Review DE solar radioastronomy; space instrumentation ID CORONAL MASS EJECTIONS; THERMAL NOISE SPECTROSCOPY; WIND ELECTRON PARAMETERS; STOCHASTIC-GROWTH THEORY; CLUMPY LANGMUIR-WAVES; EARTHS BOW SHOCK; SOLAR-WIND; 1 AU; INTERPLANETARY MEDIUM; HARMONIC EMISSION AB This paper introduces and describes the radio and plasma wave investigation on the STEREO Mission: STEREO/WAVES or S/WAVES. The S/WAVES instrument includes a suite of state-of-the-art experiments that provide comprehensive measurements of the three components of the fluctuating electric field from a fraction of a hertz up to 16 MHz, plus a single frequency channel near 30 MHz. The instrument has a direction finding or goniopolarimetry capability to perform 3D localization and tracking of radio emissions associated with streams of energetic electrons and shock waves associated with Coronal Mass Ejections (CMEs). The scientific objectives include: (i) remote observation and measurement of radio waves excited by energetic particles throughout the 3D heliosphere that are associated with the CMEs and with solar flare phenomena, and (ii) in-situ measurement of the properties of CMEs and interplanetary shocks, such as their electron density and temperature and the associated plasma waves near 1 Astronomical Unit (AU). Two companion papers provide details on specific aspects of the S/WAVES instrument, namely the electric antenna system (Bale et al., Space Sci. Rev., 2007) and the direction finding technique (Cecconi et al., Space Sci. Rev., 2007). C1 [Bougeret, J. L.; Maksimovic, M.; Monge, N.; Astier, P. L.; Davy, S.; Dekkali, M.; Manning, R. E.; Bonnin, X.; Briand, C.; Cecconi, B.; Hoang, S.; Lecacheux, A.; Mangeney, A.; Nguyen, Q. N.; Zarka, P.; Zouganelis, I.] Observ Paris, UMR CNRS 8109, LESIA, F-92195 Meudon, France. [Goetz, K.; Kellogg, P. J.; Monson, S. J.; Hinze, J. J.; Cattell, C. A.; Silvis, J. M.] Univ Minnesota, Sch Phys & Astron, Minneapolis, MN 55455 USA. [Kaiser, M. L.; Fainberg, J.; MacDowall, R. J.; Meetre, C. A.; Reiner, M. J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Bale, S. D.; Aguilar-Rodriguez, E.; Eastwood, J.; Huttunen, K. E. J.; Krucker, S.; Pulupa, M.; Salem, C.; Ullrich, R.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Bale, S. D.; Pulupa, M.] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA. [Cairns, I. H.; Robinson, P. A.] Univ Sydney, Sch Phys, Sydney, NSW 2006, Australia. [Ergun, R. E.] Univ Colorado, Atmospher & Space Phys Lab, Boulder, CO 80309 USA. [Macher, W.; Oswald, T. H.; Rucker, H.] Austrian Acad Sci, Space Res Inst, A-8010 Graz, Austria. [Moussas, X.] Univ Athens, Dept Phys, Sect Astrophys Astron & Mech, Athens, Greece. [Reiner, M. J.] Catholic Univ Amer, Washington, DC 20064 USA. [Santolik, O.] Charles Univ Prague, Fac Math & Phys, Prague, Czech Republic. [Santolik, O.] CAS, IAP, Prague, Czech Republic. RP Maksimovic, M (reprint author), Observ Paris, UMR CNRS 8109, LESIA, F-92195 Meudon, France. EM milan.maksimovic@obspm.fr RI Bale, Stuart/E-7533-2011; MacDowall, Robert/D-2773-2012; Kilpua, Emilia/G-8994-2012; Santolik, Ondrej/F-7766-2014; OI Bale, Stuart/0000-0002-1989-3596; Cattell, Cynthia/0000-0002-3805-320X; Pulupa, Marc/0000-0002-1573-7457; Cairns, Iver/0000-0001-6978-9765 NR 89 TC 188 Z9 189 U1 1 U2 9 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0038-6308 J9 SPACE SCI REV JI Space Sci. Rev. PD APR PY 2008 VL 136 IS 1-4 BP 487 EP 528 DI 10.1007/s11214-007-9298-8 PG 42 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 322OC UT WOS:000257384200016 ER PT J AU Aschwanden, MJ Burlaga, LF Kaiser, ML Ng, CK Reames, DV Reiner, MJ Gombosi, TI Lugaz, N Manchester, W IV Roussev, II Zurbuchen, TH Farrugia, CJ Galvin, AB Lee, MA Linker, JA Mikic, Z Riley, P Alexander, D Sandman, AW Cook, JW Howard, RA Odstrcil, D Pizzo, VJ Kota, J Liewer, PC Luhmann, JG Inhester, B Schwenn, RW Solanki, SK Vasyliunas, VM Wiegelmann, T Blush, L Bochsler, P Cairns, IH Robinson, PA Bothmer, V Kecskemety, K Llebaria, A Maksimovic, M Scholer, M Wimmer-Schweingruber, RF AF Aschwanden, Markus J. Burlaga, L. F. Kaiser, M. L. Ng, C. K. Reames, D. V. Reiner, M. J. Gombosi, T. I. Lugaz, N. Manchester, W., IV Roussev, I. I. Zurbuchen, T. H. Farrugia, C. J. Galvin, A. B. Lee, M. A. Linker, J. A. Mikic, Z. Riley, P. Alexander, D. Sandman, A. W. Cook, J. W. Howard, R. A. Odstrcil, D. Pizzo, V. J. Kota, J. Liewer, P. C. Luhmann, J. G. Inhester, B. Schwenn, R. W. Solanki, S. K. Vasyliunas, V. M. Wiegelmann, T. Blush, L. Bochsler, P. Cairns, I. H. Robinson, P. A. Bothmer, V. Kecskemety, K. Llebaria, A. Maksimovic, M. Scholer, M. Wimmer-Schweingruber, R. F. TI Theoretical modeling for the STEREO mission SO SPACE SCIENCE REVIEWS LA English DT Review DE STEREO mission; solar corona; solar wind; coronal mass ejection (CME); solar filaments; heliosphere; interplanetary shocks; interplanetary particle beams; solar energetic particle events (SEP); solar flares; space weather; stereoscopy; 3D reconstruction techniques; white-light emission; EUV emission; interplanetary radio emission ID CORONAL MASS EJECTIONS; SOLAR RADIO-BURSTS; ACTIVE-REGION LOOPS; SPACE WEATHER EVENT; WHITE-LIGHT IMAGES; MAGNETIC-FLUX ROPE; AB-INITIO APPROACH; GLOBAL MHD MODEL; WHOLE SUN MONTH; 3-DIMENSIONAL PROPAGATION AB We summarize the theory and modeling efforts for the STEREO mission, which will be used to interpret the data of both the remote-sensing (SECCHI, SWAVES) and in-situ instruments (IMPACT, PLASTIC). The modeling includes the coronal plasma, in both open and closed magnetic structures, and the solar wind and its expansion outwards from the Sun, which defines the heliosphere. Particular emphasis is given to modeling of dynamic phenomena associated with the initiation and propagation of coronal mass ejections (CMEs). The modeling of the CME initiation includes magnetic shearing, kink instability, filament eruption, and magnetic reconnection in the flaring lower corona. The modeling of CME propagation entails interplanetary shocks, interplanetary particle beams, solar energetic particles (SEPs), geoeffective connections, and space weather. This review describes mostly existing models of groups that have committed their work to the STEREO mission, but is by no means exhaustive or comprehensive regarding alternative theoretical approaches. C1 [Aschwanden, Markus J.] Lockheed Martin ATC, Solar & Astrophys Lab, Palo Alto, CA 94304 USA. [Burlaga, L. F.; Kaiser, M. L.; Ng, C. K.; Reames, D. V.; Reiner, M. J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Gombosi, T. I.; Lugaz, N.; Manchester, W., IV; Roussev, I. I.; Zurbuchen, T. H.] Univ Michigan, Ann Arbor, MI 48109 USA. [Farrugia, C. J.; Galvin, A. B.; Lee, M. A.] Univ New Hampshire, Durham, NH 03824 USA. [Linker, J. A.; Mikic, Z.; Riley, P.] SAIC, San Diego, CA 92121 USA. [Alexander, D.; Sandman, A. W.] Rice Univ, Dept Phys & Astron, Houston, TX 77251 USA. [Cook, J. W.; Howard, R. A.] USN, Res Lab, Washington, DC 20375 USA. [Odstrcil, D.; Pizzo, V. J.] NOAA, SEC, Boulder, CO 80303 USA. [Kota, J.] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA. [Liewer, P. C.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Luhmann, J. G.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Inhester, B.; Schwenn, R. W.; Solanki, S. K.; Vasyliunas, V. M.; Wiegelmann, T.] Max Planck Inst Sonnensyst Forsch, D-37191 Katlenburg Lindau, Germany. [Blush, L.; Bochsler, P.] Univ Bern, Inst Phys, CH-3012 Bern, Switzerland. [Cairns, I. H.; Robinson, P. A.] Univ Sydney, Sch Phys, Sydney, NSW 2006, Australia. [Bothmer, V.] Univ Gottingen, Inst Astrophys, D-37077 Gottingen, Germany. [Kecskemety, K.] HKFI RMKI, H-1525 Budapest, Hungary. [Llebaria, A.] CNRS, Astron Spatiale Lab, F-13376 Marseille, France. [Maksimovic, M.] Observ Paris, CNRS, F-92195 Meudon, France. [Maksimovic, M.] Observ Paris, LESIA, F-92195 Meudon, France. [Scholer, M.] Max Planck Inst Extraterr Phys, Ctr Interdisciplinary Plasma Sci, D-85740 Munich, Germany. [Wimmer-Schweingruber, R. F.] Univ Kiel, Phys IEAP, D-24118 Kiel, Germany. RP Aschwanden, MJ (reprint author), Lockheed Martin ATC, Solar & Astrophys Lab, 3251 Hanover St, Palo Alto, CA 94304 USA. EM aschwanden@1msa1.com RI Lugaz, Noe/C-1284-2008; Roussev, Ilia/E-9141-2011; Gombosi, Tamas/G-4238-2011; Manchester, Ward/I-9422-2012; Galvin, Antoinette/A-6114-2013; Solanki, Sami/E-2487-2013 OI Cairns, Iver/0000-0001-6978-9765; Lugaz, Noe/0000-0002-1890-6156; Gombosi, Tamas/0000-0001-9360-4951; Solanki, Sami/0000-0002-3418-8449 NR 218 TC 21 Z9 22 U1 1 U2 4 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0038-6308 EI 1572-9672 J9 SPACE SCI REV JI Space Sci. Rev. PD APR PY 2008 VL 136 IS 1-4 BP 565 EP 604 DI 10.1007/s11214-006-9027-8 PG 40 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 322OC UT WOS:000257384200019 ER PT J AU Eichstedt, J Thompson, WT Cyr, OCS AF Eichstedt, J. Thompson, W. T. Cyr, O. C. St. TI STEREO ground segment, science operations, and data archive SO SPACE SCIENCE REVIEWS LA English DT Review DE STEREO; space weather; science operations; data archive; solar observations ID SYSTEM AB Vitally important to the success of any mission is the ground support system used for commanding the spacecraft, receiving the telemetry, and processing the results. We describe the ground system used for the STEREO mission, consisting of the Mission Operations Center, the individual Payload Operations Centers for each instrument, and the STEREO Science Center, together with mission support from the Flight Dynamics Facility, Deep Space Mission System, and the Space Environment Center. The mission planning process is described, as is the data flow from spacecraft telemetry to processed science data to long-term archive. We describe the online resources that researchers will be able to use to access STEREO planning resources, science data, and analysis software. The STEREO Joint Observations Program system is described, with instructions on how observers can participate. Finally, we describe the near-real-time processing of the "space weather beacon" telemetry, which is a low telemetry rate quicklook product available close to 24 hours a day, with the intended use of space weather forecasting. C1 [Thompson, W. T.] NASA, Goddard Space Flight Ctr, Adnet Syst Inc, Greenbelt, MD 20771 USA. [Eichstedt, J.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA. RP Thompson, WT (reprint author), NASA, Goddard Space Flight Ctr, Adnet Syst Inc, Code 671, Greenbelt, MD 20771 USA. EM William.T.Thompson.1@gsfc.nasa.gov RI Thompson, William/D-7376-2012 NR 6 TC 4 Z9 4 U1 0 U2 1 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0038-6308 J9 SPACE SCI REV JI Space Sci. Rev. PD APR PY 2008 VL 136 IS 1-4 BP 605 EP 626 DI 10.1007/s11214-007-9249-4 PG 22 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 322OC UT WOS:000257384200020 ER PT J AU Peticolas, LM Craig, N Kucera, T Michels, DJ Gerulskis, J MacDowall, RJ Beisser, K Chrissotimos, C Luhmann, JG Galvin, AB Ratta, L Drobnes, E Mendez, BJ Hill, S Marren, K Howard, R AF Peticolas, L. M. Craig, N. Kucera, T. Michels, D. J. Gerulskis, J. MacDowall, R. J. Beisser, K. Chrissotimos, C. Luhmann, J. G. Galvin, A. B. Ratta, L. Drobnes, E. Mendez, B. J. Hill, S. Marren, K. Howard, R. TI The solar terrestrial relations observatory (STEREO) Education and Outreach (E/PO) program SO SPACE SCIENCE REVIEWS LA English DT Review DE education; outreach; Sun : coronal mass ejections (CMEs); Sun : magnetic fields; Sun : particle emission; Sun : solar-terrestrial relations AB The STEREO mission's Education and Outreach (E/PO) program began early enough its team benefited from many lessons learned as NASA's E/PO profession matured. Originally made up of discrete programs, by launch the STEREO E/PO program had developed into a quality suite containing all the program elements now considered standard: education workshops, teacher/student guides, national and international collaboration, etc. The benefit of bringing so many unique programs together is the resulting diverse portfolio, with scientists, E/PO professionals, and their education partners all of whom can focus on excellent smaller programs. The drawback is a less cohesive program nearly impossible to evaluate in its entirety with the given funding. When individual components were evaluated, we found our programs mostly made positive impact. In this paper, we elaborate on the programs, hoping that others will effectively use or improve upon them. When possible, we indicate the programs' effects on their target audiences. C1 [Peticolas, L. M.; Craig, N.; Luhmann, J. G.; Mendez, B. J.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Kucera, T.; MacDowall, R. J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Michels, D. J.; Howard, R.] USN, Res Lab, Ctr Space Res, Washington, DC 20375 USA. [Gerulskis, J.] Christa McAuliffe Planetarium, Concord, NH 03301 USA. [Beisser, K.; Marren, K.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA. [Chrissotimos, C.] Sci Syst & Applicat Inc, Cranbury, NJ 08512 USA. [Galvin, A. B.] Univ New Hampshire, Ctr Space Sci, Durham, NH 03824 USA. [Ratta, L.] Integrated Commun Technol Inc, Greenbelt, MD 20770 USA. [Drobnes, E.] ADNEt Syst Inc, Rockville, MD 20852 USA. [Hill, S.] RS Informat Syst, Greenbelt, MD 20771 USA. RP Peticolas, LM (reprint author), Univ Calif Berkeley, Space Sci Lab, 77 Gauss Way, Berkeley, CA 94720 USA. EM laura@ssl.berkeley.edu RI Kucera, Therese/C-9558-2012; MacDowall, Robert/D-2773-2012; OI Kucera, Therese/0000-0001-9632-447X NR 10 TC 0 Z9 0 U1 0 U2 0 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0038-6308 J9 SPACE SCI REV JI Space Sci. Rev. PD APR PY 2008 VL 136 IS 1-4 BP 627 EP 646 DI 10.1007/s11214-007-9287-y PG 20 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 322OC UT WOS:000257384200021 ER PT J AU Kohout, T Kletetschka, G Donadini, F Fuller, M Herrero-Bervera, E AF Kohout, T. Kletetschka, G. Donadini, F. Fuller, M. Herrero-Bervera, E. TI Analysis of the natural remanent magnetization of rocks by measuring the efficiency ratio through alternating field demagnetization spectra SO STUDIA GEOPHYSICA ET GEODAETICA LA English DT Article DE REM; efficiency of magnetization; coercivity; shock remanence; SRM ID DEPENDENCE; PLOTS AB The REM(AF) method is a new tool for the analysis of the origin and alternating field demagnetization coercivity spectra of the remanent magnetization. We applied this method on precambrian Gila diabase sheets from Arizona in order to identify the high coercivity magnetic carrier, and on artificially shocked Rowley Regis basalt from UK in order to analyze the effect of the shock on the natural remanent magnetization. In the Gila diabase the high coercivity magnetic component was identified to be most likely represented by the acicular magnetite (increase in the efficiency ratio in the high coercivity region). In the Rowley Regis basalt, the REM(AF) analysis revealed that comparing to NRM, the shock produced a different distribution of the AF demagnetization coercivity spectra due to the occurrence of the Shock Remanent Magnetization. C1 [Kohout, T.; Donadini, F.] Univ Helsinki, Dept Phys, Helsinki, Finland. [Kohout, T.; Donadini, F.] Charles Univ Prague, Dept Appl Geophys, Prague 12843 2, Czech Republic. [Kohout, T.; Kletetschka, G.] Acad Sci Czech Republic, Inst Geol, Prague 16500 6, Czech Republic. [Kletetschka, G.] Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA. [Kletetschka, G.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Donadini, F.] Univ Calif San Diego, Scripps Inst Oceanog, San Diego, CA 92103 USA. [Fuller, M.; Herrero-Bervera, E.] Univ Hawaii Manoa, HIGP SOEST, Honolulu, HI 96822 USA. RP Kohout, T (reprint author), Univ Helsinki, Dept Phys, POB 64, Helsinki, Finland. EM tomas.kohout@helsinki.fi RI Kohout, Tomas/C-1394-2008; Kletetschka, Gunther/C-9996-2011 OI Kohout, Tomas/0000-0003-4458-3650; Kletetschka, Gunther/0000-0002-0645-9037 NR 19 TC 2 Z9 2 U1 0 U2 7 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0039-3169 J9 STUD GEOPHYS GEOD JI Stud. Geophys. Geod. PD APR PY 2008 VL 52 IS 2 BP 225 EP 235 DI 10.1007/s11200-008-0015-1 PG 11 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 315UY UT WOS:000256906900006 ER PT J AU Adachi, T Kletetschka, G AF Adachi, T. Kletetschka, G. TI Impact-pressure controlled orientation of shatter cone magnetizations in Sierra Madera, Texas, USA SO STUDIA GEOPHYSICA ET GEODAETICA LA English DT Article DE shatter cones; demagnetization; remagnetization; impact crater; shock fractures; magnetism; magnetic efficiency; magnetic signatures; magnetic anomaly; Mars ID VREDEFORT METEORITE CRATER; SHOCK METAMORPHISM; SOUTH-AFRICA; QUARTZ; ROCKS; ORIGIN AB A suite of Sierra Madera Impact deformed rocks was studied and magnetic analyses were performed. We characterized the magnetic signatures of two locations, sites A and B that have different physical characteristics of shock fractured structures as well as the magnetic signatures. Shatter cone at site A has a fine-scale (few to similar to 10 mm) distributed array of complete shatter cones with sharp apex. Natural remanent magnetization (NRM) of site A shatter cone is distributed within the plane that is perpendicular to the apexes of the cones. Shatter cone at site B shows no apparent cone shape or apex, instead, a relatively larger scale and multiple striated joint set (MSJS) and sinusoidal continuous peak. NRM of site B shatter cone is clustered along the apexes. The difference in magnetization direction is a likely indicator of the shock pressure where parallel to apex indicates pressures larger than 10 GPa and perpendicular to apex indicate pressures less than 10 GPa. Intensities of NRM and saturation isothermal remanent magnetization (SIRM) contrast and fluctuate within a shatter cone as well as in between two sites. We observed a random orientation of magnetic vector directions and amplitudes changing over small scales leading to the absence of coherent macro-scale signature. C1 [Adachi, T.; Kletetschka, G.] Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA. [Adachi, T.; Kletetschka, G.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Kletetschka, G.] Acad Sci Czech Republic, Inst Geol, Prague 16500 6, Czech Republic. RP Adachi, T (reprint author), Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA. EM tomoko.adachi@ssedmail.gsfc.nasa.gov RI Kletetschka, Gunther/C-9996-2011 OI Kletetschka, Gunther/0000-0002-0645-9037 NR 27 TC 2 Z9 2 U1 0 U2 9 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0039-3169 J9 STUD GEOPHYS GEOD JI Stud. Geophys. Geod. PD APR PY 2008 VL 52 IS 2 BP 237 EP 254 DI 10.1007/s11200-008-0016-0 PG 18 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 315UY UT WOS:000256906900007 ER PT J AU Andersen, O Berry, P Freeman, J Lemoine, FG Lutsckhe, S Jakobsen, F Butts, M AF Andersen, Ole Berry, Philippa Freeman, Jennifer Lemoine, Frank G. Lutsckhe, S. Jakobsen, Flemming Butts, Michael TI Satellite altimetry and GRACE gravimetry for studies of annual water storage variations in Bangladesh SO TERRESTRIAL ATMOSPHERIC AND OCEANIC SCIENCES LA English DT Article; Proceedings Paper CT International Workshop on Coast and Land Applications of Satellite Altimetry CY JUL 21-22, 2006 CL Beijing, PEOPLES R CHINA SP Chinese Acad Surveying & Mapping, Natl Chiao Tung Univ, Asia GIS & GPS Co, Chung Hsing Surv Co, Huanyu Surv Engn Cons, Real World Engn Cons DE altimetry; grace; river-level; ground water ID GRAVITY-FIELD AB Four different data sources have been compared with respect to observations of the annual water storage variations in the region of Bangladesh. Data from satellite altimeters and river gauges estimates the variation in surface water storage in the major rivers of Bangladesh. The GRACE satellites measure the integrated mass change and hence the terrestrial soil moisture variations, which can also be estimated by a hydrological model (GLDAS). These types of observations enable the derivation of the integrated water storage in the entire region of Bangladesh. For all data types, the annual signal has been estimated from a common dataset spanning the period 2003 and 2004. All four different data observe that water storage in Bangladesh is largely dominated by an annual signal with a phase peaking in early September. The annual variations in river level peaks roughly two weeks earlier than terrestrial soil moisture observations by GRACE observations and GLDAS model output. C1 [Andersen, Ole] DTU, Danish Natl Space Ctr, DK-2100 Copenhagen, Denmark. [Berry, Philippa; Freeman, Jennifer] De Montfort Univ, EAPRS Lab, Leicester LE1 9BH, Leics, England. [Lemoine, Frank G.; Lutsckhe, S.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Jakobsen, Flemming; Butts, Michael] DHI Water & Environm, DK-2970 Horsholm, Denmark. RP Andersen, O (reprint author), DTU, Danish Natl Space Ctr, DK-2100 Copenhagen, Denmark. EM oa@space.dtu.dk RI Lemoine, Frank/D-1215-2013; Andersen, Ole /H-7481-2016 OI Andersen, Ole /0000-0002-6685-3415 NR 15 TC 10 Z9 12 U1 2 U2 10 PU CHINESE GEOSCIENCE UNION PI TAIPEI PA PO BOX 23-59, TAIPEI 10764, TAIWAN SN 1017-0839 J9 TERR ATMOS OCEAN SCI JI Terr. Atmos. Ocean. Sci. PD APR PY 2008 VL 19 IS 1-2 BP 47 EP 52 DI 10.3319/TAO.2008.19.1-2.47(SA) PG 6 WC Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences; Oceanography SC Geology; Meteorology & Atmospheric Sciences; Oceanography GA 300WQ UT WOS:000255856500005 ER PT J AU Bauschlicher, CW Lawson, JW AF Bauschlicher, Charles W., Jr. Lawson, John W. TI Current-voltage curves for molecular junctions: the issue of the basis set for the metal contacts SO THEORETICAL CHEMISTRY ACCOUNTS LA English DT Article DE DFT; Greens Functions; current-voltage curves; molecular electronics ID EFFECTIVE CORE POTENTIALS; ELECTRONIC DEVICES; CONDUCTANCE; FORMALISM; TRANSPORT; EXCHANGE; ENERGY; WIRES AB We present current-voltage (I-V) curves for a chain of six Au atoms and for benzene-1,4-dithiol between two Au (111) surfaces computed using a self-consistent, non-equilibrium, Green's Functions approach in conjunction with a density functional theory (DFT) description of the extended molecule. The solutions are expanded in Gaussian basis sets. In an attempt to improve the description of the molecule-surface bond, we consider one- and two-layer clusters of metal atoms in the extended molecule. To avoid non-physical charging of the bulk metal clusters we add a shift to the diagonal elements of the Fock Matrix of the metal atoms in the DFT treatment; this can be viewed as correcting the self-energies or shifting the Fermi level. The Au-6 cluster with the full minimal basis set represents a compromise between accuracy and cost. The Au-31(12/19) two-layer cluster results are of about the same quality as the one-layer Au-21 cluster, but allows one to study more binding sites. Using a double zeta basis set for three of the top-layer Au atoms of the Au-31(12/19) cluster yields result similar to the all minimal basis set, while using all double zeta atoms yields inferior results. C1 [Bauschlicher, Charles W., Jr.; Lawson, John W.] NASA, Ames Res Ctr, Ctr Adv Mat & Devices, Moffett Field, CA 94035 USA. RP Bauschlicher, CW (reprint author), NASA, Ames Res Ctr, Ctr Adv Mat & Devices, Mail Stop 230-3, Moffett Field, CA 94035 USA. EM Charles.W.Bauschlicher@nasa.gov; John.W.Lawson@nasa.gov NR 30 TC 1 Z9 1 U1 1 U2 5 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 1432-881X J9 THEOR CHEM ACC JI Theor. Chem. Acc. PD APR PY 2008 VL 119 IS 5-6 BP 429 EP 435 DI 10.1007/s00214-007-0398-z PG 7 WC Chemistry, Physical SC Chemistry GA 280DY UT WOS:000254406400003 ER PT J AU Kehrer, K Graf, B Roeder, WP AF Kehrer, Kristen Graf, Brian Roeder, William P. TI Global positioning system (GPS) precipitable water in forecasting lightning at Spaceport Canaveral SO WEATHER AND FORECASTING LA English DT Article ID VAPOR AB This paper evaluates the use of precipitable water (PW) from the global positioning system (GPS) in lightning prediction. Additional independent verification of an earlier model is performed. This earlier model used binary logistic regression with the following four predictor variables optimally selected from a candidate list of 23 candidate predictors: the current precipitable water value for a given time of the day, the change in GPS PW over the past 9 h, the K index, and the electric field mill value. The K index was used as a measure of atmospheric stability, which, of the traditional stability measures, has been shown to work best in the area and season under study. This earlier model was not optimized for any specific forecast interval, but showed promise for 6- and 1.5-h forecasts. Two new models were developed and verified. These new models were optimized for two operationally significant forecast intervals. The first model was optimized for the 0.5-h lightning advisories issued by the U. S. Air Force's 45th Weather Squadron. An additional 1.5 h was allowed for sensor dwell, communication, calculation, analysis, and advisory decision by the forecaster. Therefore, the 0.5-h advisory model became a 2-h forecast model for lightning within the 45th Weather Squadron advisory areas. The second model was optimized for major ground processing operations supported by the 45th Weather Squadron, which can require lightning forecasts with a lead time of up to 7.5 h. Using the same 1.5-h lag as in the other new model, this became a 9-h forecast model for lightning within 37 km (20 n mi) of the 45th Weather Squadron advisory areas. The two new models were built using binary logistic regression and a list of 26 candidate predictor variables: the current GPS PW value, the K index, and 24 candidate variables of the change in GPS PW levels over 0.5-h increments up to 12 h. The new 2-h model found the following four predictors to be statistically significant, listed in decreasing order of contribution to the forecast: the 0.5-h change in GPS PW, the 7.5-h change in GPS PW, the current GPS PW value, and the K index. The new 9-h forecast model found the following five independent variables to be statistically significant, listed in decreasing order of contribution to the forecast: the current GPS PW value, the 8.5-h change in GPS PW, the 3.5-h change in GPS PW, the 12-h change in GPS PW, and the K index. In both models, the GPS PW parameters had better correlation to the lightning forecast than did the K index, a widely used thunderstorm index. Possible future improvements to this study are discussed. C1 [Kehrer, Kristen; Graf, Brian] NASA, Kennedy Space Ctr, FL 32899 USA. [Roeder, William P.] Patrick AFB, Miami, FL USA. RP Kehrer, K (reprint author), NASA, Mail Stop EA-C, Kennedy Space Ctr, FL 32899 USA. EM kristen.c.kehrer@nasa.gov NR 19 TC 2 Z9 2 U1 1 U2 1 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 0882-8156 J9 WEATHER FORECAST JI Weather Forecast. PD APR PY 2008 VL 23 IS 2 BP 219 EP 232 DI 10.1175/2007WAF2006105.1 PG 14 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 289TT UT WOS:000255077500002 ER PT J AU Herring, GC Popovic, S AF Herring, G. C. Popovic, S. TI Microwave air breakdown enhanced with metallic initiators SO APPLIED PHYSICS LETTERS LA English DT Article ID DISCHARGE AB We have determined X-band (9.4 GHz) electric field strengths required to obtain air breakdown at atmospheric pressure in the presence of metallic initiators, which are irradiated with repetitive (30 pulses/s) microwave pulses of 3 mu s duration and 200 kW peak power. Using a half-wavelength initiator, a factor of 40 reduction (compared to no initiator) was observed in the electric field required to achieve breakdown. The present measurements are compared to a previously published model for air breakdown, which was originally validated with S-band (3 GHz) frequencies and single 40 mu s pulses. We find good agreement between this previous model and our present measurements of breakdown with X-band frequencies and repetitive 3 mu s pulses. (C) 2008 American Institute of Physics. C1 [Herring, G. C.] NASA, Langley Res Ctr, Hampton, VA 23681 USA. [Popovic, S.] Old Dominion Univ, Dept Phys, Norfolk, VA 23529 USA. RP Herring, GC (reprint author), NASA, Langley Res Ctr, Hampton, VA 23681 USA. EM gregory.c.herring@nasa.gov NR 11 TC 4 Z9 5 U1 0 U2 1 PU AMER INST PHYSICS PI MELVILLE PA CIRCULATION & FULFILLMENT DIV, 2 HUNTINGTON QUADRANGLE, STE 1 N O 1, MELVILLE, NY 11747-4501 USA SN 0003-6951 J9 APPL PHYS LETT JI Appl. Phys. Lett. PD MAR 31 PY 2008 VL 92 IS 13 AR 131501 DI 10.1063/1.2897308 PG 3 WC Physics, Applied SC Physics GA 283XN UT WOS:000254669900020 ER PT J AU Correira, J Aikin, AC Grebowsky, JM Pesnell, WD Burrows, JP AF Correira, J. Aikin, A. C. Grebowsky, J. M. Pesnell, W. D. Burrows, J. P. TI Seasonal variations of magnesium atoms in the mesosphere-thermosphere SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID UPPER-ATMOSPHERE; POTASSIUM LAYER; IONOSPHERE; MODEL; IRON; IONS; MG; CHEMISTRY; ARECIBO; MIDDLE AB UV radiances from the Global Ozone Monitoring Experiment (GOME) spectrometer on the ERS-2 satellite are used to determine long-term dayside temporal variations of the total vertical column density below 795 km of the meteoric metal species Mg and Mg+ in the upper atmosphere. The GOME instrument has the ability to observe the ground state transition lines of Mg I at 285.2 nm and resolve the Mg II at 280 nm. A retrieval algorithm has been developed to determine column densities and applied to the years 1996-1997. Results show the middle latitude dayside Mg+ peaks in total vertical content during the summer, while neutral Mg demonstrates a much more subtle maximum in summer. Dayside trends are opposite previous midlatitude nighttime lidar observations, with the exception of calcium. The Mg+/Mg ratio has a seasonal variation, reaching a maximum in the summer. The total content of Mg+ is twice that of neutral Mg. C1 [Correira, J.; Aikin, A. C.] Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA. [Grebowsky, J. M.; Pesnell, W. D.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Burrows, J. P.] Univ Bremen, Inst Environm Phys, D-28359 Bremen, Germany. RP Correira, J (reprint author), Catholic Univ Amer, Dept Phys, 200 Hannan Hall,620 Michigan Ave NE, Washington, DC 20064 USA. EM john.correira@gmail.com; aikin@comcast.net; joseph.m.grebowsky@nasa.gov; william.d.pesnell@nasa.gov RI Pesnell, William/D-1062-2012; Grebowsky, Joseph/I-7185-2013; Burrows, John/B-6199-2014 OI Pesnell, William/0000-0002-8306-2500; Burrows, John/0000-0002-6821-5580 NR 34 TC 8 Z9 8 U1 0 U2 6 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 EI 1944-8007 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD MAR 29 PY 2008 VL 35 IS 6 AR L06103 DI 10.1029/2007GL033047 PG 6 WC Geosciences, Multidisciplinary SC Geology GA 281XM UT WOS:000254532200003 ER PT J AU Fan, CJ Schulze-Makuch, D Fairen, AG Wolff, JA AF Fan, Chaojun Schulze-Makuch, Dirk Fairen, Alberto G. Wolff, John A. TI A new hypothesis for the origin and redistribution of sulfates in the equatorial region of western Mars SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID MERIDIANI-PLANUM; OMEGA/MARS EXPRESS; MARTIAN CLIMATE; LANDING SITE; SULFUR; SPECTROMETER; DEPOSITS; BASALT; OCEANS; CRATER AB The formation of sulfates on Mars has been under debate since they were identified by several Mars missions starting from the 1970s. We propose that sulfates formed as evaporites in enclosed standing bodies of water in the Valles Marineris area following the early alteration of Martian basaltic crust, were then elevated by the Tharsis uplift, and transported together with rock materials to Meridiani Planum by periodic outbursts of water, where they were deposited as sediments. The proposed model comprehensively addresses all forms of sulfate occurrences near the equator in the western Martian hemisphere and relates it to physiographic processes (volcanic, tectonic and sedimentary) affecting the Martian surface. C1 [Fan, Chaojun; Schulze-Makuch, Dirk; Wolff, John A.] Washington State Univ, Sch Earth & Environm Sci, Pullman, WA 99164 USA. [Fairen, Alberto G.] NASA, Ames Res Ctr, Space Sci & Astrobiol Div, Moffett Field, CA 94035 USA. RP Fan, CJ (reprint author), Washington State Univ, Sch Earth & Environm Sci, Pullman, WA 99164 USA. EM cfan1@wsu.edu RI Fan, Chaojun/A-9966-2010; OI Schulze-Makuch, Dirk/0000-0002-1923-9746 NR 42 TC 8 Z9 8 U1 1 U2 1 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD MAR 29 PY 2008 VL 35 IS 6 AR L06201 DI 10.1029/2007GL033079 PG 5 WC Geosciences, Multidisciplinary SC Geology GA 281XM UT WOS:000254532200004 ER PT J AU Ma, Q Tipping, RH Leforestier, C AF Ma, Q. Tipping, R. H. Leforestier, C. TI Temperature dependences of mechanisms responsible for the water-vapor continuum absorption. I. Far wings of allowed lines SO JOURNAL OF CHEMICAL PHYSICS LA English DT Article ID POTENTIAL FUNCTIONS; ROTATIONAL BANDS; LIQUID WATER; SHAPE THEORY; CM-1; H2O; CO2; SPECTROSCOPY; REGION; ENERGY AB It is well known that the water-vapor continuum plays an important role in the radiative balance in the Earth's atmosphere. This was first discovered by Elsasser almost 70 years ago, and since that time there has been a large body of work, both experimental and theoretical, on this topic. It has been experimentally shown that for ambient atmospheric conditions, the continuum absorption scales quadratically with the H(2)O number density and has a strong, negative temperature dependence (T dependence). Over the years, there have been three different theoretical mechanisms postulated: Far wings of allowed transitions, water dimers, and collision-induced absorption. Despite the improvements in experimental data, at present there is no consensus on which mechanism is primarily responsible for the absorption. The first mechanism proposed was the accumulation of the far-wing absorption of the strong allowed transitions. Later, absorption by water dimers was proposed and this mechanism provides a qualitative explanation for the strong, negative T dependence. Recently, some atmospheric modelers have proposed that collision-induced absorption is one of the major contributors. However, based on improvements in the theoretical calculation of accurate far-wing line shapes, ab initio dimer calculations, and theoretical collision-induced absorptions, it is now generally accepted that the dominant mechanism for the absorption in the infrared (IR) windows is that due to the far wings. Whether this is true for other spectral regions is not presently established. Although all these three mechanisms have a negative T dependence, their T dependences will be characterized by individual features. To analyze the characteristics of the latter will enable one to assess their roles with more certainty. In this paper, we present a detailed study of the T dependence of the far-wing absorption mechanism. We will then compare our theoretical calculations with the most recent and accurate experimental data in the IR windows. The results of our calculations are found to agree very well with measurements in the 800-1200 cm(-1) region. We conclude from this work that the T dependence in the IR window region predicted by the far-wing theory is negative and moderately strong. Its pattern is not simple and it could vary significantly as the frequency of interest varies. (C) 2008 American Institute of Physics. C1 [Ma, Q.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA. [Ma, Q.] Columbia Univ, Dept Appl Phys & Appl Math, New York, NY 10025 USA. [Tipping, R. H.] Univ Alabama, Dept Phys & Astron, Tuscaloosa, AL 35487 USA. [Leforestier, C.] Univ Montpellier 2, CNRS, UMR, CC 1501, F-34095 Montpellier, France. RP Ma, Q (reprint author), NASA, Goddard Inst Space Studies, 2880 Broadway, New York, NY 10025 USA. EM qma@giss.nasa.gov NR 38 TC 31 Z9 38 U1 1 U2 3 PU AMER INST PHYSICS PI MELVILLE PA CIRCULATION & FULFILLMENT DIV, 2 HUNTINGTON QUADRANGLE, STE 1 N O 1, MELVILLE, NY 11747-4501 USA SN 0021-9606 J9 J CHEM PHYS JI J. Chem. Phys. PD MAR 28 PY 2008 VL 128 IS 12 AR 124313 DI 10.1063/1.2839604 PG 17 WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical SC Chemistry; Physics GA 281ZK UT WOS:000254537200026 PM 18376925 ER PT J AU Seo, KW Wilson, CR Han, SC Waliser, DE AF Seo, K. W. Wilson, C. R. Han, S. C. Waliser, D. E. TI Gravity Recovery and Climate Experiment (GRACE) alias error from ocean SO JOURNAL OF GEOPHYSICAL RESEARCH-SOLID EARTH LA English DT Article ID GRAVIMETRY; TIDES; MODEL AB Gravity Recovery and Climate Experiment (GRACE) is able to observe interannual and longer-period mass redistribution driven by climate changes. However, alias errors due to inaccurate ocean tide models may contaminate these signals. To quantify this problem, we estimate alias contamination due to expected errors in eight tidal constituents (Q(1), O-1, P-1, K-1, N-2, M-2, S-2, and K-2) for the period August 2002 to February 2006. Differences between GOT00.2 and TPXO6.2 tide models are used as estimates of tide model errors. The alias estimate is based on an approximate method employing least squares fits of spherical harmonics to potential differences between the two GRACE satellites. Results from this method are similar to previous estimates, confirming this is a useful and efficient way to study the alias problem. New findings are (1) the period of the M2 tide alias is about 140 d, much longer than the predicted period (13.5 d) because of monthly sampling of the 13.5-d period; (2) there are two alias periods for K1 (one about (0 d and one longer than 7 years); and (3) the slow decay in the GRACE orbit causes tide component aliases to differ from pure frequencies as the orbit evolves. We also find that aliases can contaminate in both space and time and thus may affect estimates of mass changes over land. Finally, we compare the simulated S2 alias with the estimated S2 alias in GRACE data. They are similar, but our approximate method appears to overestimate alias error over high-latitude oceans and along certain coastlines while underestimating error over low-latitude oceans. C1 [Seo, K. W.; Waliser, D. E.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Wilson, C. R.] Univ Texas Austin, Jackson Sch Geosci, Dept Geol Sci, Austin, TX 78712 USA. [Han, S. C.] Ohio State Univ, Sch Earth Sci, Columbus, OH 43210 USA. RP Seo, KW (reprint author), Korea Polar Res Inst, 504 Get Pearl Tower, Inchon 406840, South Korea. RI Han, Shin-Chan/A-2022-2009 NR 20 TC 17 Z9 20 U1 1 U2 2 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 MAR 28 PY 2008 VL 113 IS B3 AR B03405 DI 10.1029/2006JB004747 PG 10 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 281YF UT WOS:000254534100001 ER PT J AU Gjerloev, JW Hoffman, RA Sigwarth, JB Frank, LA Baker, JBH AF Gjerloev, J. W. Hoffman, R. A. Sigwarth, J. B. Frank, L. A. Baker, J. B. H. TI Typical auroral substorm: A bifurcated oval SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article ID HEIGHT-INTEGRATED CONDUCTIVITY; UV; MORPHOLOGY; IMAGER; SYSTEM; SECTOR; ARCS; DMSP AB Utilizing global auroral images obtained by Polar Visible Imaging System Earth Camera, we have analyzed the UV emissions from 116 auroral substorms. The events selected were fairly isolated and had to expand from a localized onset. It was found that essentially all auroral events fulfilling these simple criteria expand into the Akasofu (1964) bulge-type aurora. Averaged auroral emission patterns were compiled for 11 time steps of the substorm covering 20 min prior to the onset until well into the recovery phase. This compilation required a three-step normalization technique, one temporal based on the expansion time and two spatial, magnetic local time and latitude. These average patterns were then fit to either a single or double Gaussian distribution in latitude for each of 24 magnetic local times. On the basis of this analysis we made the following conclusions. The normalization technique is highly efficient in maintaining the key features in the individual auroral emission patterns, even though the individual events varied significantly in intensity, size, position, and lifetime. Thus our normalization results quantitatively validate the Akasofu (1964) assumption that key auroral features exist in the bulge-type auroral substorm. After the substorm onset the auroral oval becomes clearly bifurcated consisting of two components: the oval aurora in the latitude range of the preonset oval and expanding primarily eastward postmidnight, and the bulge aurora, which emerges out of the oval, expanding poleward and both east and west in MLT. The oval aurora decay faster than the bulge emissions indicating that the decays have separate time constants. Owing to the pronounced difference in the spatiotemporal behavior of the two auroral components we suggest that their sources are quasi-independent. C1 [Gjerloev, J. W.; Baker, J. B. H.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA. [Hoffman, R. A.] NASA, Goddard Space Flight Ctr, Space Weather Lab, Greenbelt, MD 20771 USA. [Sigwarth, J. B.] NASA, Goddard Space Flight Ctr, Div Off, Heliophys Div, Greenbelt, MD 20771 USA. [Frank, L. A.] Univ Iowa, Dept Phys & Astron, Iowa City, IA 52242 USA. RP Gjerloev, JW (reprint author), Johns Hopkins Univ, Appl Phys Lab, Johns Hopkins Rd, Laurel, MD 20723 USA. EM jesper.gjerloev@jhuapl.edu NR 33 TC 11 Z9 12 U1 1 U2 3 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9380 EI 2169-9402 J9 J GEOPHYS RES-SPACE JI J. Geophys. Res-Space Phys. PD MAR 28 PY 2008 VL 113 IS A3 AR A03211 DI 10.1029/2007JA012431 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 281YI UT WOS:000254534400001 ER PT J AU Araneda, JA Marsch, E Vinas, AF AF Araneda, Jaime A. Marsch, Eckart Vinas, Adolfo F. - TI Proton core heating and beam formation via parametrically unstable Alfven-cyclotron waves SO PHYSICAL REVIEW LETTERS LA English DT Article ID SOLAR-WIND; VELOCITY DISTRIBUTIONS; PLASMA AB Vlasov theory and one-dimensional hybrid simulations are used to study the effects that compressible fluctuations driven by parametric instabilities Alfven-cyclotron waves have on proton velocity distributions. Field-aligned proton beams are generated during the saturation phase of the wave-particle interaction, with a drift speed which is slightly greater than the Alfven speed and is maintained until the end of the simulation. The main part of the distribution becomes anisotropic due to phase mixing as is typically observed in the velocity distributions measured in the fast solar wind. We identify the key instabilities and also find that, even in the parameter regime where fluid theory appears to be appropriate, strong kinetic effects still prevail. C1 [Araneda, Jaime A.] Univ Concepcion, Dept Fis, Concepcion 4070386, Chile. [Marsch, Eckart] Max Planck Inst, Sonnensyst Forsch, D-37191 Katlenburg Lindau, Germany. [Vinas, Adolfo F. -] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Araneda, JA (reprint author), Univ Concepcion, Dept Fis, Concepcion 4070386, Chile. EM jaraneda@udec.cl RI Araneda, Jaime/J-9245-2015 NR 28 TC 88 Z9 88 U1 0 U2 3 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 0031-9007 J9 PHYS REV LETT JI Phys. Rev. Lett. PD MAR 28 PY 2008 VL 100 IS 12 AR 125003 DI 10.1103/PhysRevLett.100.125003 PG 4 WC Physics, Multidisciplinary SC Physics GA 281CK UT WOS:000254473800038 PM 18517877 ER PT J AU Dyudina, UA Ingersoll, AP Ewald, SP Vasavada, AR West, RA Del Genio, AD Barbara, JM Porco, CC Achterberg, RK Flasar, FM Simon-Miller, AA Fletcher, LN AF Dyudina, Ulyana A. Ingersoll, Andrew P. Ewald, Shawn P. Vasavada, Ashwin R. West, Robert A. Del Genio, Anthony D. Barbara, John M. Porco, Carolyn C. Achterberg, Richard K. Flasar, F. Michael Simon-Miller, Amy A. Fletcher, Leigh N. TI Dynamics of Saturn's south polar vortex SO SCIENCE LA English DT Article C1 [Dyudina, Ulyana A.; Ingersoll, Andrew P.; Ewald, Shawn P.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. [Vasavada, Ashwin R.; West, Robert A.; Fletcher, Leigh N.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Del Genio, Anthony D.; Barbara, John M.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA. [Porco, Carolyn C.] Space Sci Inst, Boulder, CO 80301 USA. [Achterberg, Richard K.; Flasar, F. Michael; Simon-Miller, Amy A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Fletcher, Leigh N.] Univ Oxford, Dept Phys, Clarendon Lab, Oxford OX1 3PU, England. RP Dyudina, UA (reprint author), CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. EM ulyana@gps.caltech.edu RI Fletcher, Leigh/D-6093-2011; Flasar, F Michael/C-8509-2012; Del Genio, Anthony/D-4663-2012; Simon, Amy/C-8020-2012 OI Fletcher, Leigh/0000-0001-5834-9588; Del Genio, Anthony/0000-0001-7450-1359; Simon, Amy/0000-0003-4641-6186 NR 5 TC 19 Z9 19 U1 1 U2 4 PU AMER ASSOC ADVANCEMENT SCIENCE PI WASHINGTON PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 USA SN 0036-8075 J9 SCIENCE JI Science PD MAR 28 PY 2008 VL 319 IS 5871 BP 1801 EP 1801 DI 10.1126/science.1153633 PG 1 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 279ZF UT WOS:000254394000039 PM 18369142 ER PT J AU Gavriil, FP Gonzalez, ME Gotthelf, EV Kaspi, VM Livingstone, MA Woods, PM AF Gavriil, F. P. Gonzalez, M. E. Gotthelf, E. V. Kaspi, V. M. Livingstone, M. A. Woods, P. M. TI Magnetar-like emission from the young pulsar in Kes 75 SO SCIENCE LA English DT Article ID X-RAY PULSAR; SOFT GAMMA-REPEATERS; TRANSIENT MAGNETAR; XTE J1810-197; RADIO PULSARS; NEUTRON-STARS; SPIN-DOWN; BURSTS; FIELD; 1E-1048.1-5937 AB We report the detection of magnetar- like x- ray bursts from the young pulsar PSR J1846- 0258, at the center of the supernova remnant Kes 75. This pulsar, long thought to be exclusively rotation- powered, has an inferred surface dipolar magnetic field of 4.9 x 10(13) gauss, which is higher than those of the vast majority of rotation- powered pulsars, but lower than those of the approximately 12 previously identified magnetars. The bursts were accompanied by a sudden flux increase and an unprecedented change in timing behavior. These phenomena lower the magnetic and rotational thresholds associated with magnetar- like behavior and suggest that in neutron stars there exists a continuum of magnetic activity that increases with inferred magnetic field strength. C1 [Gavriil, F. P.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Gavriil, F. P.] Univ Maryland Baltimore Cty, Ctr Res & Explorat Space Sci & Technol, Baltimore, MD 21250 USA. [Gonzalez, M. E.; Kaspi, V. M.; Livingstone, M. A.] McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada. [Gotthelf, E. V.] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA. [Kaspi, V. M.; Woods, P. M.] Dynetics, Huntsville, AL 35806 USA. [Woods, P. M.] Natl Space Sci & Technol Ctr, Huntsville, AL 35805 USA. RP Gavriil, FP (reprint author), NASA, Goddard Space Flight Ctr, Code 662, Greenbelt, MD 20771 USA. EM fotis.p.gavriil@nasa.gov NR 30 TC 113 Z9 113 U1 0 U2 1 PU AMER ASSOC ADVANCEMENT SCIENCE PI WASHINGTON PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 USA SN 0036-8075 J9 SCIENCE JI Science PD MAR 28 PY 2008 VL 319 IS 5871 BP 1802 EP 1805 DI 10.1126/science.1153465 PG 4 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 279ZF UT WOS:000254394000040 PM 18292305 ER PT J AU Livesey, NJ Filipiak, MJ Froidevaux, L Read, WG Lambert, A Santee, ML Jiang, JH Pumphrey, HC Waters, JW Cofield, RE Cuddy, DT Daffer, WH Drouin, BJ Fuller, RA Jarnot, RF Jiang, YB Knosp, BW Li, QB Perun, VS Schwartz, MJ Snyder, WV Stek, PC Thurstans, RP Wagner, PA Avery, M Browell, EV Cammas, JP Christensen, LE Diskin, GS Gao, RS Jost, HJ Loewenstein, M Lopez, JD Nedelec, P Osterman, GB Sachse, GW Webster, CR AF Livesey, N. J. Filipiak, M. J. Froidevaux, L. Read, W. G. Lambert, A. Santee, M. L. Jiang, J. H. Pumphrey, H. C. Waters, J. W. Cofield, R. E. Cuddy, D. T. Daffer, W. H. Drouin, B. J. Fuller, R. A. Jarnot, R. F. Jiang, Y. B. Knosp, B. W. Li, Q. B. Perun, V. S. Schwartz, M. J. Snyder, W. V. Stek, P. C. Thurstans, R. P. Wagner, P. A. Avery, M. Browell, E. V. Cammas, J. -P. Christensen, L. E. Diskin, G. S. Gao, R. -S. Jost, H. -J. Loewenstein, M. Lopez, J. D. Nedelec, P. Osterman, G. B. Sachse, G. W. Webster, C. R. TI Validation of Aura Microwave Limb Sounder O-3 and CO observations in the upper troposphere and lower stratosphere SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID MOZAIC AIRBORNE PROGRAM; DIAL MEASUREMENTS; WATER-VAPOR; EOS MLS; OZONE; TRANSPORT; AIRCRAFT; AIR; RETRIEVAL; SATELLITE AB Global satellite observations of ozone and carbon monoxide from the Microwave Limb Sounder (MLS) on the EOS Aura spacecraft are discussed with emphasis on those observations in the 215-100 hPa region (the upper troposphere and lower stratosphere). The precision, resolution and accuracy of the data produced by the MLS "version 2.2'' processing algorithms are discussed and quantified. O-3 accuracy is estimated at similar to 40 ppbv + 5% (similar to 20 ppbv + 20% at 215 hPa) while the CO accuracy is estimated at similar to 30 ppbv + 30% for pressures of 147 hPa and less. Comparisons with expectations and other observations show good agreements for the O3 product, generally consistent with the systematic errors quoted above. In the case of CO, a persistent factor of similar to 2 high bias is seen at 215 hPa. However, the morphology is shown to be realistic, consistent with raw MLS radiance data, and useful for scientific study. The MLS CO data at higher altitudes are shown to be consistent with other observations. C1 [Livesey, N. J.; Froidevaux, L.; Read, W. G.; Lambert, A.; Santee, M. L.; Jiang, J. H.; Waters, J. W.; Cofield, R. E.; Cuddy, D. T.; Daffer, W. H.; Drouin, B. J.; Fuller, R. A.; Jarnot, R. F.; Jiang, Y. B.; Knosp, B. W.; Li, Q. B.; Perun, V. S.; Schwartz, M. J.; Snyder, W. V.; Stek, P. C.; Thurstans, R. P.; Wagner, P. A.; Christensen, L. E.; Osterman, G. B.; Webster, C. R.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Filipiak, M. J.; Pumphrey, H. C.] Univ Edinburgh, Sch Geosci, Edinburgh EH8 9YL, Midlothian, Scotland. [Avery, M.; Browell, E. V.; Diskin, G. S.; Sachse, G. W.] NASA, Langley Res Ctr, Hampton, VA 23681 USA. [Cammas, J. -P.; Nedelec, P.] CNRS, UMR5560, Lab Aerol, F-31400 Toulouse, France. [Gao, R. -S.] NOAA, Div Chem Sci, Earth Syst Res Lab, Boulder, CO 80305 USA. [Jost, H. -J.] Novawave Technol, Redwood City, CA 94065 USA. [Loewenstein, M.; Lopez, J. D.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Livesey, NJ (reprint author), CALTECH, Jet Prop Lab, Mail Stop 183-701, Pasadena, CA 91109 USA. EM nathaniel.j.livesey@jpl.nasa.gov RI Gao, Ru-Shan/H-7455-2013; Schwartz, Michael/F-5172-2016; Manager, CSD Publications/B-2789-2015 OI Schwartz, Michael/0000-0001-6169-5094; NR 35 TC 122 Z9 124 U1 2 U2 11 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 MAR 27 PY 2008 VL 113 IS D15 AR D15S02 DI 10.1029/2007JD008805 PG 15 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 281XS UT WOS:000254532800001 ER PT J AU Tzortziou, M Krotkov, NA Cede, A Herman, JR Vasilkov, A AF Tzortziou, Maria Krotkov, Nickolay A. Cede, Alexander Herman, Jay R. Vasilkov, Alexander TI A new technique for retrieval of tropospheric and stratospheric ozone profiles using sky radiance measurements at multiple view angles: Application to a Brewer spectrometer SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID AEROSOL OPTICAL DEPTH; SHADOW-BAND RADIOMETER; DOBSON SPECTROPHOTOMETERS; O-3 PROFILES; RADIATIVE-TRANSFER; SATELLITE DATA; UV IRRADIANCE; LIDAR; GOME; VARIABILITY AB This paper describes and applies a new technique for retrieving diurnal variability in tropospheric ozone vertical distribution using ground-based measurements of ultraviolet sky radiances. The measured radiances are obtained by a polarization-insensitive modified Brewer double spectrometer located at Goddard Space Flight Center, in Greenbelt, Maryland, USA. Results demonstrate that the Brewer angular (0-72 degrees viewing zenith angle) and spectral (303-320 nm) measurements of sky radiance in the solar principal plane provide sufficient information to derive tropospheric ozone diurnal variability. In addition, the Brewer measurements provide stratospheric ozone vertical distributions at least twice per day near sunrise and sunset. Frequent measurements of total column ozone amounts from direct-sun observations are used as constraints in the retrieval. The vertical ozone profile resolution is shown in terms of averaging kernels to yield at least four points in the troposphere-low stratosphere, including good information in Umkehr layer 0 (0-5 km). The focus of this paper is on the derivation of stratospheric and tropospheric ozone profiles using both simulated and measured radiances. We briefly discuss the necessary modifications of the Brewer spectrometer that were used to eliminate instrumental polarization sensitivity so that accurate sky radiances can be obtained in the presence of strong Rayleigh scattering and aerosols. The results demonstrate that including a site-specific and time-dependent aerosol correction, based on Brewer direct-sun observations of aerosol optical thickness, is critical to minimize the sky radiance residuals as a function of observing angle in the optimal estimation inversion algorithm and improve the accuracy of the retrieved ozone profile. C1 [Tzortziou, Maria; Cede, Alexander] Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20742 USA. [Tzortziou, Maria; Krotkov, Nickolay A.; Cede, Alexander; Herman, Jay R.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Krotkov, Nickolay A.] Univ Maryland, Goddard Earth Sci & Technol Ctr, Baltimore, MD 21201 USA. [Vasilkov, Alexander] Sci Syst & Applicat Inc, Lanham, MD USA. RP Tzortziou, M (reprint author), Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20742 USA. EM maria.a.tzortziou@nasa.gov RI Krotkov, Nickolay/E-1541-2012; OI Krotkov, Nickolay/0000-0001-6170-6750; Herman, Jay/0000-0002-9146-1632 NR 49 TC 3 Z9 3 U1 0 U2 5 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 MAR 27 PY 2008 VL 113 IS D6 AR D06304 DI 10.1029/2007JD009093 PG 14 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 281XP UT WOS:000254532500001 ER PT J AU Davila, AF Gomez-Silva, B de los Rios, A Ascaso, C Olivares, H Mckay, CP Wierzchos, J AF Davila, Alfonso F. Gomez-Silva, Benito de los Rios, Asuncion Ascaso, Carmen Olivares, Hector Mckay, Christopher P. Wierzchos, Jacek TI Facilitation of endolithic microbial survival in the hyperarid core of the Atacama Desert by mineral deliquescence SO JOURNAL OF GEOPHYSICAL RESEARCH-BIOGEOSCIENCES LA English DT Article ID WATER RELATIONS; PHOTOSYNTHESIS; MARS; CHROOCOCCIDIOPSIS; METEORITES; CHILE; LIFE AB The hyperarid core of the Atacama Desert is considered the dry limit for life on Earth. Soils in this region have very low abundance of heterotrophic bacteria and are practically barren of photosynthetic microorganisms because of the extreme dry conditions (<= 2 mm a(-1) rainfall). However, relatively abundant endolithic communities of cyanobacteria (Chroococcidiopsis) occur within halite crusts in paleolake evaporitic deposits. By means of continuous monitoring of the microclimate conditions ( temperature, relative humidity, water vapor density, wetness, and photosynthetically active radiation) inside and around the halite crusts, we demonstrate here that water vapor condenses within the pore space of the halite at relative humidity ( RH) levels that otherwise hinder the occurrence of liquid water in the surrounding environment. Water condensation occurs at RH > 75%, which corresponds to the deliquescence point of halite. We have estimated a total of 57 deliquescence events (i.e., water condensation) within the halite crusts, as opposed to only 1 liquid water event outside. These wet events resulted in a total of 213.8 h of potential photosynthetic activity for the endolithic microorganisms versus only 6 h for organisms outside the halite crusts. Halite crusts may therefore represent the last available niche for photosynthetic activity in extreme arid environments on Earth. C1 [Davila, Alfonso F.; Mckay, Christopher P.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Gomez-Silva, Benito; Olivares, Hector] Univ Antofagasta, Dept Biomed, Antofagasta, Chile. [Gomez-Silva, Benito; Olivares, Hector] Univ Antofagasta, Inst Desierto, Antofagasta, Chile. [de los Rios, Asuncion; Ascaso, Carmen] CSIC, CCMA, Inst Recursos Nat, E-28006 Madrid, Spain. [Wierzchos, Jacek] Univ Lleida, Serv Microscopia Elect, E-25198 Lleida, Spain. RP Davila, AF (reprint author), NASA, Ames Res Ctr, MS 245-3,Moffett Field, Moffett Field, CA 94035 USA. EM alfonso.fernandez-davila-1@nasa.gov RI Wierzchos, Jacek/F-7036-2011; Ascaso, Carmen/F-5369-2011; Davila, Alfonso/A-2198-2013; de los Rios, Asuncion/L-3694-2014 OI Wierzchos, Jacek/0000-0003-3084-3837; Ascaso, Carmen/0000-0001-9665-193X; Davila, Alfonso/0000-0002-0977-9909; de los Rios, Asuncion/0000-0002-0266-3516 NR 21 TC 61 Z9 62 U1 4 U2 30 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 MAR 27 PY 2008 VL 113 IS G1 AR G01028 DI 10.1029/2007JG000561 PG 9 WC Environmental Sciences; Geosciences, Multidisciplinary SC Environmental Sciences & Ecology; Geology GA 281XU UT WOS:000254533000001 ER PT J AU Styers-Barnett, DJ Ellison, SP Mehl, BP Westlake, BC House, RL Park, C Wise, KE Papanikolas, JM AF Styers-Barnett, David J. Ellison, Stephen P. Mehl, Brian P. Westlake, Brittany C. House, Ralph L. Park, Cheol Wise, Kristopher E. Papanikolas, John M. TI Exciton dynamics and biexciton formation in single-walled carbon nanotubes studied with femtosecond transient absorption spectroscopy SO JOURNAL OF PHYSICAL CHEMISTRY C LA English DT Article ID SEMICONDUCTOR QUANTUM DOTS; OPTICAL SPECTROSCOPY; ULTRAFAST RELAXATION; CARRIER DYNAMICS; RAMAN-SCATTERING; POLYMER; STATES; MOLECULES; CHEMISTRY; KINETICS AB We used femtosecond transient absorption (TA) spectroscopy to examine the excited state dynamics of single-walled carbon nanotube (SWNT) bundles embedded in polymer matrices. The SWNTs were excited by a femtosecond pump pulse centered at either 1800, 900, or 550 nm and probed using a white-light continuum extending from 400 to 750 nm. We observed a structured TA spectrum consisting of a series of narrow induced transmission (IT) and induced absorption (IA) bands. The TA spectrum, which is independent of excitation wavelength, appeared on a time scale shorter than our instrument response (200 fs) and persisted for up to 100 ps. TA spectra obtained at a series of pump-probe delay times provided a window through which to monitor the exciton dynamics. We observed three distinct spectral signatures in the time-dependent data: (1) the decay of a broad photobleach, (2) the biphasic decay of narrow IT and IA features, and (3) a dynamical spectral shift of IA bands. These processes were attributed to plasmon relaxation, electron-hole recombination, and lattice relaxation associated with exciton self-trapping, respectively. Analysis of the transient spectrum suggested that it arose from a nonlinear optical response of the SWNT, where excitons produced by the pump pulse modified the transition frequencies of subsequent carrier excitations. The result was a series of IT bands (bleaches) at the ground state absorption frequencies, and associated with each was a corresponding red-shifted absorption band. These induced absorptions were attributed to the formation of biexcitons, four-particle excitations that are produced through the sequential excitation of two closely spaced electron-hole pairs. C1 [Styers-Barnett, David J.; Ellison, Stephen P.; Mehl, Brian P.; Westlake, Brittany C.; House, Ralph L.; Papanikolas, John M.] Univ N Carolina, Dept Chem, Venable & Kenan Labs, Chapel Hill, NC 27599 USA. [Park, Cheol; Wise, Kristopher E.] NASA, Langley Res Ctr, Natl Inst Aerosp, Hampton, VA 23681 USA. RP Papanikolas, JM (reprint author), Univ N Carolina, Dept Chem, Venable & Kenan Labs, CB 3290, Chapel Hill, NC 27599 USA. EM John_Papanikolas@unc.edu NR 86 TC 32 Z9 33 U1 3 U2 44 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 MAR 27 PY 2008 VL 112 IS 12 BP 4507 EP 4516 DI 10.1021/jp7099256 PG 10 WC Chemistry, Physical; Nanoscience & Nanotechnology; Materials Science, Multidisciplinary SC Chemistry; Science & Technology - Other Topics; Materials Science GA 290FM UT WOS:000255108700014 ER PT J AU Bhushan, B Galasso, B Bignardi, C Nguyen, CV Dai, LM Qu, LT AF Bhushan, Bharat Galasso, Barbara Bignardi, Cristina Nguyen, Cattien V. Dai, Liming Qu, Liangti TI Adhesion, friction and wear on the nanoscale of MWNT tips and SWNT and MWNT arrays SO NANOTECHNOLOGY LA English DT Article ID SCANNING PROBE MICROSCOPY; CARBON NANOTUBE FILMS; CERAMIC-MATRIX NANOCOMPOSITES; ATOMIC-FORCE MICROSCOPY; FIELD-EMISSION; TRIBOLOGICAL PROPERTIES; POLYMER COMPOSITES; LATERAL RESOLUTION; AFM PROBES; FABRICATION AB The nanotribological characterization of carbon nanotubes is fundamental for the exploration of new sliding applications. In this study, a comprehensive investigation of adhesion, friction and wear of a multiwalled nanotube (MWNT) tip, and SWNT (single-walled nanotube) and MWNT arrays has been carried out. A nonlinear response of the MWNT tip is observed when the tip is brought into and out of contact with various surfaces. A nonlinear response occurs due to the buckling of the nanotube and its subsequent sliding on the surface. In addition to the role of surface chemistry, it can also explain the relatively high value of the coefficient of friction obtained on different surfaces, as compared to that of Si and Si(3)N(4) tips. The adhesion and friction studies carried out on SWNT and MWNT arrays using Si tips show that SWNT arrays, compared to MWNT arrays, exhibit lower values, possibly due to lower van der Waals forces as a result of lower packing density and higher flexibility. The wear tests conducted with the MWNT tip and a Si tip on a gold film, at two normal loads, show less damage of the surface when the MWNT tip is used because of the MWNT acting as a compliant spring, absorbing part of the load. Wear tests conducted with a Si tip on SWNT and MWNT arrays show that the arrays do not wear. The tip wear and the friction force in the SWNT array are lower, because of lower adhesion and higher flexibility of the SWNTs, which causes less opposition to the motion of the tip. C1 [Bhushan, Bharat] Ohio State Univ, Nanotribol Lab Informat Storage, Columbus, OH 43210 USA. [Bhushan, Bharat] Ohio State Univ, MEMS NEMS, Columbus, OH 43210 USA. [Galasso, Barbara; Bignardi, Cristina] Politecn Torino, Dipartimento Meccan, I-10129 Turin, Italy. [Nguyen, Cattien V.] NASA, Ames Res Ctr, ELORET, Moffett Field, CA 94035 USA. [Dai, Liming; Qu, Liangti] Univ Dayton, Res Inst, Dept Chem & Mat Engn, Dayton, OH 45469 USA. RP Bhushan, B (reprint author), Ohio State Univ, Nanotribol Lab Informat Storage, 201 W 19th Ave, Columbus, OH 43210 USA. RI Bhushan, Bharat/A-9684-2013 OI Bhushan, Bharat/0000-0001-7161-6601 NR 69 TC 13 Z9 13 U1 4 U2 16 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0957-4484 J9 NANOTECHNOLOGY JI Nanotechnology PD MAR 26 PY 2008 VL 19 IS 12 AR 125702 DI 10.1088/0957-4484/19/12/125702 PG 10 WC Nanoscience & Nanotechnology; Materials Science, Multidisciplinary; Physics, Applied SC Science & Technology - Other Topics; Materials Science; Physics GA 276WK UT WOS:000254174200024 PM 21817743 ER PT J AU Ho, CM Morabito, DD Woo, R AF Ho, C. M. Morabito, D. D. Woo, R. TI Solar corona effects on angle of arrival fluctuations for microwave telecommunication links during superior solar conjunction SO RADIO SCIENCE LA English DT Article AB During the superior solar conjunction of spacecraft, the transmitted signals from a spacecraft to the Earth ground station graze the region near the Sun's photospheric surface, passing through dense and turbulent regions of solar-charged particles. Phase changes due to solar coronal irregularities cause raypath wandering, wavefront tilting, and fluctuations in the apparent angle of arrival when observed from the Earth. This study presents a first theoretical investigation of solar wind and solar coronal effects on the angle of arrival fluctuations for RF signals. On the basis of the Chandrasekhar relationship between phase and angular fluctuations, an analytical integrating solution for angle of arrival fluctuations is derived by applying solar corona and plasma irregularity spectrum models. It is found that angular fluctuations rapidly decrease with increasing heliocentric distance at a rate of similar to r(-5.5) and also decrease with increasing frequency at a rate of similar to 1/f(2). It is found that when using K(a) band at alpha = 0.4 degrees (r = 1.6 solar radii), there is a 19 millidegrees (mdeg) angular scattering, corresponding to a 9 dB gain degradation. In comparison, lower-frequency X and S band signals undergo much worse degradation effects. Beyond alpha = 2 degrees (r > 8 solar radii), angular fluctuations at microwave frequency bands can almost be neglected (theta(RMS) < 1 mdeg). A solution to minimize this degradation is to use K(a)- or higher-frequency bands for the telecommunication link during periods of solar conjunction. This study not only quantifies the angular fluctuations caused by solar corona irregularities but also provides an effective method for diagnosing the plasma density fluctuations in a region very close to the solar photospheric surface. C1 [Ho, C. M.; Morabito, D. D.; Woo, R.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Ho, CM (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM cmho@mail.jpl.nasa.gov NR 16 TC 2 Z9 2 U1 0 U2 1 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0048-6604 J9 RADIO SCI JI Radio Sci. PD MAR 26 PY 2008 VL 43 IS 2 AR RS2003 DI 10.1029/2007RS003620 PG 13 WC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology & Atmospheric Sciences; Remote Sensing; Telecommunications SC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology & Atmospheric Sciences; Remote Sensing; Telecommunications GA 281YM UT WOS:000254534800001 ER PT J AU Anderson, MS AF Anderson, Mark S. TI Nearfield surface enhanced spectroscopy using targeted nanoparticle deposition SO APPLIED PHYSICS LETTERS LA English DT Article ID ATOMIC-FORCE MICROSCOPE; RAMAN-SCATTERING; FIELD AB Surface enhanced spectroscopy is demonstrated by depositing gold nanoparticles on a surface using an atomic force microscope. A modified dip pen nanolithography process is used to place particles directly on to a target. Near-field optical enhancement is demonstrated for Raman and infrared spectroscopies and is applicable for fluorescence spectroscopy. This approach provides localized, near-field spectroscopy with subdiffraction limit resolution and a general method for fabricating plasmonic device structures. (C) 2008 American Institute of Physics. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Anderson, MS (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM mark.s.anderson@jpl.nasa.gov NR 16 TC 13 Z9 13 U1 0 U2 5 PU AMER INST PHYSICS PI MELVILLE PA CIRCULATION & FULFILLMENT DIV, 2 HUNTINGTON QUADRANGLE, STE 1 N O 1, MELVILLE, NY 11747-4501 USA SN 0003-6951 J9 APPL PHYS LETT JI Appl. Phys. Lett. PD MAR 24 PY 2008 VL 92 IS 12 AR 123101 DI 10.1063/1.2891085 PG 3 WC Physics, Applied SC Physics GA 281PJ UT WOS:000254510300072 ER PT J AU Hubbard, SM Cress, CD Bailey, CG Raffaelle, RP Bailey, SG Wilt, DM AF Hubbard, S. M. Cress, C. D. Bailey, C. G. Raffaelle, R. P. Bailey, S. G. Wilt, D. M. TI Effect of strain compensation on quantum dot enhanced GaAs solar cells SO APPLIED PHYSICS LETTERS LA English DT Article ID INTERMEDIATE BAND AB GaP tensile strain compensation ( SC ) layers were introduced into GaAs solar cells enhanced with a five layer stack of InAs quantum dots (QDs ). One sun air mass zero illuminated current- voltage curves show that SC results in improved conversion efficiency and reduced dark current. The strain compensated QD solar cell shows a slight increase in short circuit current compared to a baseline GaAs cell due to sub- GaAs bandgap absorption by the InAs QD. Quantum efficiency and electroluminescence were also measured and provide further insight to the improvements due to SC. (C) 2008 American Institute of Physics. C1 [Hubbard, S. M.; Cress, C. D.; Bailey, C. G.; Raffaelle, R. P.] Rochester Inst Technol, Nanopower Res Lab, Dept Phys, Rochester, NY 14623 USA. [Bailey, S. G.; Wilt, D. M.] NASA, Glenn Res Ctr, Photovolta & Power Technol Branch, Cleveland, OH 44135 USA. RP Hubbard, SM (reprint author), Rochester Inst Technol, Nanopower Res Lab, Dept Phys, 85 Lomb Mem Dr, Rochester, NY 14623 USA. EM smhsps@rit.edu RI Cress, Cory/A-8673-2009; OI Cress, Cory/0000-0001-7563-6693 NR 19 TC 228 Z9 228 U1 6 U2 64 PU AMER INST PHYSICS PI MELVILLE PA CIRCULATION & FULFILLMENT DIV, 2 HUNTINGTON QUADRANGLE, STE 1 N O 1, MELVILLE, NY 11747-4501 USA SN 0003-6951 J9 APPL PHYS LETT JI Appl. Phys. Lett. PD MAR 24 PY 2008 VL 92 IS 12 AR 123512 DI 10.1063/1.2903699 PG 3 WC Physics, Applied SC Physics GA 281PJ UT WOS:000254510300099 ER PT J AU Kumar, S Gao, J Zmuidzinas, J Mazin, BA Leduc, HG Day, PK AF Kumar, Shwetank Gao, Jiansong Zmuidzinas, Jonas Mazin, Benjamin A. LeDuc, Henry G. Day, Peter K. TI Temperature dependence of the frequency and noise of superconducting coplanar waveguide resonators SO APPLIED PHYSICS LETTERS LA English DT Article ID KINETIC INDUCTANCE DETECTORS; MICROWAVE SQUID MULTIPLEXER; PHOTON; CAVITY; QUBIT AB We present measurements of the temperature and power dependence of the resonance frequency and frequency noise of superconducting niobium thin-film coplanar waveguide resonators carried out at temperatures well below the superconducting transition (T-c=9.2 K). The noise decreases by nearly two orders of magnitude as the temperature is increased from 120 to 1200 mK, while the variation of the resonance frequency with temperature over this range agrees well with the standard two-level system (TLS) model for amorphous dielectrics. These results support the hypothesis that TLSs are responsible for the noise in superconducting microresonators and have important implications for resonator applications such as qubits and photon detectors. (C) 2008 American Institute of Physics. C1 [Kumar, Shwetank; Gao, Jiansong; Zmuidzinas, Jonas; Mazin, Benjamin A.] CALTECH, Div Phys Math & Astron, Pasadena, CA 91125 USA. [LeDuc, Henry G.; Day, Peter K.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Kumar, S (reprint author), CALTECH, Div Phys Math & Astron, Pasadena, CA 91125 USA. EM jonas@caltech.edu RI Mazin, Ben/B-8704-2011 OI Mazin, Ben/0000-0003-0526-1114 NR 28 TC 35 Z9 35 U1 1 U2 10 PU AMER INST PHYSICS PI MELVILLE PA 1305 WALT WHITMAN RD, STE 300, MELVILLE, NY 11747-4501 USA SN 0003-6951 EI 1077-3118 J9 APPL PHYS LETT JI Appl. Phys. Lett. PD MAR 24 PY 2008 VL 92 IS 12 AR 123503 DI 10.1063/1.2894584 PG 3 WC Physics, Applied SC Physics GA 281PJ UT WOS:000254510300090 ER PT J AU Vallisneri, M Crowder, J Tinto, M AF Vallisneri, Michele Crowder, Jeff Tinto, Massimo TI Sensitivity and parameter-estimation precision for alternate LISA configurations SO CLASSICAL AND QUANTUM GRAVITY LA English DT Article AB We describe a simple framework to assess the LISA scientific performance (more specifically, its sensitivity and expected parameter-estimation precision for prescribed gravitational-wave signals) under the assumption of failure of one or two inter-spacecraft laser measurements (links) and of one to four intra-spacecraft laser measurements. We apply the framework to the simple case of measuring the LISA sensitivity to monochromatic circular binaries, and the LISA parameter-estimation precision for the gravitational-wave polarization angle of these systems. Compared to the six-link baseline configuration, the five-link case is characterized by a small loss in signal-to-noise ratio (SNR) in the high-frequency section of the LISA band; the four-link case shows a reduction by a factor of root 2 at low frequencies, and by up to similar to 2 at high frequencies. The uncertainty in the estimate of polarization, as computed in the Fisher-matrix formalism, also worsens when moving from six to five, and then to four links: this can be explained by the reduced SNR available in those configurations (except for observations shorter than three months, where five and six links do better than four even with the same SNR). In addition, we prove (for generic signals) that the SNR and Fisher matrix are invariant with respect to the choice of a basis of TDI observables; rather, they depend only on which inter-spacecraft and intra-spacecraft measurements are available. C1 [Vallisneri, Michele; Crowder, Jeff; Tinto, Massimo] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Vallisneri, M (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM Michele.Vallisneri@jpl.nasa.gov NR 24 TC 12 Z9 12 U1 1 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0264-9381 J9 CLASSICAL QUANT GRAV JI Class. Quantum Gravity PD MAR 21 PY 2008 VL 25 IS 6 AR 065005 DI 10.1088/0264-9381/25/6/065005 PG 17 WC Astronomy & Astrophysics; Physics, Multidisciplinary; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA 276OA UT WOS:000254150700006 ER PT J AU Ajello, JM Gustin, J Stewart, I Larsen, K Esposito, L Pryor, W McClintock, W Stevens, MH Malone, CP Dziczek, D AF Ajello, Joseph M. Gustin, Jacques Stewart, Ian Larsen, Kristopher Esposito, Larry Pryor, Wayne McClintock, William Stevens, Michael H. Malone, Charles P. Dziczek, Dariusz TI Titan airglow spectra from the Cassini Ultraviolet Imaging Spectrograph: FUV disk analysis SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID ELECTRON-IMPACT; INFRARED OBSERVATIONS; VOYAGER-1 ENCOUNTER; EUV EMISSION; ATMOSPHERE; SYSTEM AB We present a spectral analysis of the far ultraviolet (FUV: 1150-1900 angstrom) disk airglow observations of Titan's atmosphere by the Cassini Ultraviolet Imaging Spectrograph (UVIS). The FUV spectrum consists of emissions from the Lyman-Birge-Hopfield (LBH) band system of N-2 excited by photoelectrons (a (1)Pi(g) -> X (1)Sigma(+)(g)), N I multiplets from solar photodissociative excitation of N-2, resonantly scattered solar H Ly-alpha and sunlight reflected by N-2 in the mesosphere-stratosphere and modified by aerosols (e. g., tholins) and hydrocarbon absorption. Below 1450 angstrom, the strongest emissions arise from H Ly-a with an intensity of 208 Rayleighs (R), LBH bands with an intensity of 43 R, and the N I multiplets with a combined intensity of 16 R. Above 1450 angstrom, most of the UVIS signal is due to reflected sunlight. Mixing ratios of tholins, C2H2, C2H4 and C4H2 have been derived from the reflected sunlight using a Rayleigh scattering model. The derived mixing ratios are in good agreement with Voyager infrared observations and with FUV photochemical models, assuming solar energy deposition above 1450 angstrom occurs near 250 km (Wilson and Atreya, 2004). We also present the first geometric albedo measurement of Titan from 1500-1900 angstrom. C1 [Ajello, Joseph M.; Malone, Charles P.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Dziczek, Dariusz] Nicholas Copernicus Univ, PL-87100 Torun, Poland. [Gustin, Jacques; Stewart, Ian; Larsen, Kristopher; Esposito, Larry; McClintock, William] Univ Colorado, Atmospher & Space Phys Lab, Boulder, CO 80303 USA. [Pryor, Wayne] Cent Arizona Coll, Dept Sci, Coolidge, AZ 85228 USA. [Stevens, Michael H.] Natl Res Lab, Space Sci Div, Washington, DC 20375 USA. RP Ajello, JM (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM joseph.m.ajello@jpl.nasa.gov RI Malone, Charles/A-6294-2010; Dziczek, Dariusz/G-3620-2014; OI Malone, Charles/0000-0001-8418-1539; Stevens, Michael/0000-0003-1082-8955 NR 26 TC 28 Z9 28 U1 1 U2 4 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 EI 1944-8007 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD MAR 21 PY 2008 VL 35 IS 6 AR L06102 DI 10.1029/2007GL032315 PG 5 WC Geosciences, Multidisciplinary SC Geology GA 281TO UT WOS:000254522000002 ER PT J AU Ajello, JM Aguilar, A Mangina, RS James, GK Geissler, P Trafton, L AF Ajello, Joseph M. Aguilar, Alejandro Mangina, Rao S. James, Geoffrey K. Geissler, Paul Trafton, Laurence TI Middle UV to near-IR spectrum of electron-excited SO2 SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Article ID ULTRAVIOLET IMAGING SPECTROSCOPY; CROSS-SECTIONS; IOS ATMOSPHERE; ATOMIC OXYGEN; O-I; IMPACT; EMISSION; EXCITATION; MODEL; HYDROGEN AB We investigated the electron impact-induced fluorescence spectrum of SO2 to provide excitation cross sections for modeling Io's emission spectrum and analyzing Cassini Imaging Science Subsystem observations. The electron-excited middle-ultraviolet visible optical near-infrared (VOIR) emission spectrum of SO2 gas was generated in the laboratory and studied from 2000 to 11,000 angstrom at a resolution of Delta lambda similar to 2.5 angstrom full width at half maximum (FWHM). The VOIR laboratory spectrum longward of 6000 angstrom consists entirely of S I, II and O I, II multiplets for electron impact energies above similar to 15 eV. Between 2000 and 6000 angstrom, we find previously identified molecular bands from both SO and SO2. This work represents a significant improvement in spectral resolution over our earlier work done at 18 angstrom FWHM. From a measurement of the medium-resolution spectrum, we provide detailed 25- and 100-eV emission cross sections for spectral features from 2000 to 11,000 angstrom. On the basis of these data, we suggest future ground-based and satellite telescopic observations in the VOIR that are of promise for understanding Io's atmosphere. C1 [Ajello, Joseph M.; Aguilar, Alejandro; Mangina, Rao S.; James, Geoffrey K.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Geissler, Paul] US Geol Survey, Flagstaff, AZ 86001 USA. [Trafton, Laurence] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA. RP Ajello, JM (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM geoffrey.james@jpl.nasa.gov NR 37 TC 4 Z9 4 U1 0 U2 0 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9097 EI 2169-9100 J9 J GEOPHYS RES-PLANET JI J. Geophys. Res.-Planets PD MAR 21 PY 2008 VL 113 IS E3 AR E03002 DI 10.1029/2007JE002921 PG 15 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 281VC UT WOS:000254526000001 ER PT J AU Ziaeepour, H Holland, ST Boyd, PT Page, K Oates, S Markwardt, CB Meszaros, P Gehrels, N Marshall, FE Cummings, J Goad, M AF Ziaeepour, Houri Holland, Stephen T. Boyd, Patricia T. Page, Kim Oates, Samantha Markwardt, Craig B. Meszaros, Peter Gehrels, Neil Marshall, Francis E. Cummings, Jay Goad, Mike TI GRB 060607A: a gamma-ray burst with bright asynchronous early X-ray and optical emissions SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE shock waves; gamma-rays : bursts ID SWIFT XRT DATA; ULTRARELATIVISTIC SHOCKS; PARTICLE-ACCELERATION; RELATIVISTIC SHOCKS; SPECTRAL EVOLUTION; WEIBEL INSTABILITY; AFTERGLOW EMISSION; FERMI ACCELERATION; TEMPORAL STRUCTURE; ROBOTIC TELESCOPE AB The early optical emission of the moderately high redshift (z = 3.08) GRB 060607A shows a remarkable broad and strong peak with a rapid rise and a relatively slow power-law decay. It is not coincident with the strong early-time flares seen in the X-ray and gamma-ray energy bands. There is weak evidence for variability superposed on this dominant component in several optical bands that can be related to flares in high-energy bands. While for a small number of gamma-ray bursts (GRBs), well-sampled optical flares have been observed simultaneously with X-ray and gamma-ray pulses, GRB 060607A is one of the few cases where the early optical emission shows no significant evidence for correlation with the prompt emission. In this work we first report in detail the broad-band observations of this burst by Swift. Then by applying a simple model for the dynamics and the synchrotron radiation of a relativistic shock, we show that the dominant component of the early emissions in optical wavelengths has the same origin as the tail emission produced after the main gamma-ray activity. The most plausible explanation for the peak in the optical light curve seems to be the cooling of the prompt after the main collisions, shifting the characteristic synchrotron frequency to the optical bands. The fact that the early emission in X-ray does not show a steep decay, like what is observed in many other GRBs, is further evidence for slow cooling of the prompt shell within this GRB. It seems that the cooling process requires a steepening of the electron energy distribution and/or a break in this distribution at high energies. From simultaneous gamma-ray emission during the first flare, the behaviour of hardness ratio, and the lack of spectral features, we conclude that the X-ray flares are due to the collision of late shells rather than late reprocessing of the central engine activities. The sharp break in the X-ray light curve at few thousands of seconds after the trigger, is not observed in the infrared/optical/ultraviolet bands, and therefore cannot be a jet break. Either the X-ray break is due to a change in the spectrum of the accelerated electrons or the lack of an optical break is due to the presence of a related delayed response component. C1 [Ziaeepour, Houri; Oates, Samantha] Mullard Space Sci Lab, Dorking RH5 6NT, Surrey, England. [Holland, Stephen T.; Gehrels, Neil] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA. [Holland, Stephen T.] Univ Space Res Assoc, Columbia, MD 21044 USA. [Holland, Stephen T.; Marshall, Francis E.; Cummings, Jay] NASA, Goddard Space Flight Ctr, CRESST, Greenbelt, MD 20771 USA. [Boyd, Patricia T.; Markwardt, Craig B.] NASA, Goddard Space Flight Ctr, Lab Astroparticle Phys, Greenbelt, MD 20771 USA. [Page, Kim; Goad, Mike] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England. [Meszaros, Peter] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. RP Ziaeepour, H (reprint author), Mullard Space Sci Lab, Dorking RH5 6NT, Surrey, England. EM hz@mssl.ucl.ac.uk RI Boyd, Patricia/D-3274-2012; Gehrels, Neil/D-2971-2012 NR 85 TC 18 Z9 18 U1 0 U2 0 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD MAR 21 PY 2008 VL 385 IS 1 BP 453 EP 467 DI 10.1111/j.1365-2966.2008.12859.x PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 287KR UT WOS:000254916500036 ER PT J AU Rodgers, SD Charnley, SB AF Rodgers, S. D. Charnley, S. B. TI Nitrogen superfractionation in dense cloud cores SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE astrochemistry; molecular processes; meteors, meteoriods; ISM : molecules ID INTERPLANETARY DUST PARTICLES; ISOTOPIC COMPOSITION; INTERSTELLAR CLOUDS; DISSOCIATIVE RECOMBINATION; GAS TEMPERATURE; ORGANIC-MATTER; STAR-FORMATION; FRACTIONATION; METEORITES; ABUNDANCES AB We report new calculations of interstellar N-15-fractionation. Previously, we have shown that large enhancements of N-15/N-14 can occur in cold, dense gas where CO is frozen out, but that the existence of an NH + N channel in the dissociative recombination of N2H+ severely curtails the fractionation. In the light of recent experimental evidence that this channel is in fact negligible, we have reassessed the N-15 chemistry in dense cloud cores. We consider the effects of temperatures below 10 K, and of the presence of large amounts of atomic nitrogen. We also show how the temporal evolution of gas-phase isotope ratios is preserved as spatial heterogeneity in ammonia ice mantles, as monolayers deposited at different times have different isotopic compositions. We demonstrate that the upper layers of this ice may have N-15/N-14 ratios an order of magnitude larger than the underlying elemental value. Converting our ratios to delta-values, we obtain delta N-15 > 3000% in the uppermost layer, with values as high as 10 000% in some models. We suggest that this material is the precursor to the N-15 'hotspots' recently discovered in meteorites and IDPs. C1 NASA, Ames Res Ctr, Div Space Sci & Astrobiol, Moffett Field, CA 94035 USA. RP Rodgers, SD (reprint author), NASA, Ames Res Ctr, Div Space Sci & Astrobiol, MS 245-3, Moffett Field, CA 94035 USA. EM rogers@dusty.arc.nasa.gov RI Charnley, Steven/C-9538-2012 NR 37 TC 48 Z9 48 U1 0 U2 5 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD MAR 21 PY 2008 VL 385 IS 1 BP L48 EP L52 DI 10.1111/j.1745-3933.2008.00431.x PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 287KR UT WOS:000254916500055 ER PT J AU Sotin, C Tobie, G AF Sotin, Christophe Tobie, Gabriel TI Planetary science - Titan's hidden ocean SO SCIENCE LA English DT Editorial Material C1 [Sotin, Christophe] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Tobie, Gabriel] Univ Nantes, Lab Planetol & Geodynam, F-44322 Nantes, France. RP Sotin, C (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM csotin@jpl.nasa.gov; gabriel.tobie@univ-nantes.fr NR 7 TC 12 Z9 13 U1 1 U2 4 PU AMER ASSOC ADVANCEMENT SCIENCE PI WASHINGTON PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 USA SN 0036-8075 J9 SCIENCE JI Science PD MAR 21 PY 2008 VL 319 IS 5870 BP 1629 EP 1630 DI 10.1126/science.1155964 PG 2 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 276VR UT WOS:000254172300028 PM 18356514 ER PT J AU Lorenz, RD Stiles, BW Kirk, RL Allison, MD del Marmo, PP Iess, L Lunine, JI Ostro, SJ Hensley, S AF Lorenz, Ralph D. Stiles, Bryan W. Kirk, Randolph L. Allison, Michael D. del Marmo, Paolo Persi Iess, Luciano Lunine, Jonathan I. Ostro, Steven J. Hensley, Scott TI Titan's rotation reveals an internal ocean and changing zonal winds SO SCIENCE LA English DT Article ID GALILEAN SATELLITES; SURFACE AB Cassini radar observations of Saturn's moon Titan over several years show that its rotational period is changing and is different from its orbital period. The present- day rotation period difference from synchronous spin leads to a shift of similar to 0.36 per year in apparent longitude and is consistent with seasonal exchange of angular momentum between the surface and Titan's dense superrotating atmosphere, but only if Titan's crust is decoupled from the core by an internal water ocean like that on Europa. C1 [Lorenz, Ralph D.] Johns Hopkins Univ, Appl Phys Lab, Dept Space, Laurel, MD 20723 USA. [Stiles, Bryan W.; Ostro, Steven J.; Hensley, Scott] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Kirk, Randolph L.] US Geol Survey, Flagstaff, AZ 86001 USA. [Allison, Michael D.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA. [del Marmo, Paolo Persi; Iess, Luciano] Univ Roma La Sapienza, I-00184 Rome, Italy. [Lunine, Jonathan I.] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA. RP Lorenz, RD (reprint author), Johns Hopkins Univ, Appl Phys Lab, Dept Space, Johns Hopkins Rd, Laurel, MD 20723 USA. EM ralph.lorenz@jhuapl.edu RI IESS, Luciano/F-4902-2011; Lorenz, Ralph/B-8759-2016 OI IESS, Luciano/0000-0002-6230-5825; Lorenz, Ralph/0000-0001-8528-4644 FU Intramural NIH HHS NR 23 TC 114 Z9 116 U1 3 U2 12 PU AMER ASSOC ADVANCEMENT SCIENCE PI WASHINGTON PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 USA SN 0036-8075 J9 SCIENCE JI Science PD MAR 21 PY 2008 VL 319 IS 5870 BP 1649 EP 1651 DI 10.1126/science.1151639 PG 3 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 276VR UT WOS:000254172300035 PM 18356521 ER PT J AU Reichle, RH Crow, WT Keppenne, CL AF Reichle, Rolf H. Crow, Wade T. Keppenne, Christian L. TI An adaptive ensemble Kalman filter for soil moisture data assimilation SO WATER RESOURCES RESEARCH LA English DT Article ID ERROR COVARIANCE PARAMETERS; LAND DATA ASSIMILATION; ALGORITHM; IMPACT AB In a 19- year twin experiment for the Red- Arkansas river basin we assimilate synthetic surface soil moisture retrievals into the NASA Catchment land surface model. We demonstrate how poorly specified model and observation error parameters affect the quality of the assimilation products. In particular, soil moisture estimates from data assimilation are sensitive to observation and model error variances and, for very poor input error parameters, may even be worse than model estimates without data assimilation. Estimates of surface heat fluxes and runoff are at best marginally improved through the assimilation of surface soil moisture and tend to have large errors when the assimilation system operates with poor input error parameters. We present a computationally affordable, adaptive assimilation system that continually adjusts model and observation error parameters in response to internal diagnostics. The adaptive filter can identify model and observation error variances and provide generally improved assimilation estimates when compared to the non- adaptive system. C1 [Reichle, Rolf H.; Keppenne, Christian L.] NASA, Goddard Space Flight Ctr, Global Modeling & Assimilat Off, Greenbelt, MD 20771 USA. [Crow, Wade T.] USDA ARS, Hydrol & Remote Sensing Lab, Beltsville, MD USA. [Reichle, Rolf H.] Univ Maryland Baltimore Cty, Goddard Earth Sci & Technol Ctr, Baltimore, MD 21228 USA. [Keppenne, Christian L.] Sci Applicat Int Corp, Beltsville, MD USA. RP Reichle, RH (reprint author), NASA, Goddard Space Flight Ctr, Global Modeling & Assimilat Off, Code 610-1,8800 Greenbelt Rd, Greenbelt, MD 20771 USA. EM rolf.reichle@nasa.gov RI Reichle, Rolf/E-1419-2012 NR 33 TC 88 Z9 88 U1 2 U2 17 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0043-1397 EI 1944-7973 J9 WATER RESOUR RES JI Water Resour. Res. PD MAR 21 PY 2008 VL 44 IS 3 AR W03423 DI 10.1029/2007WR006357 PG 13 WC Environmental Sciences; Limnology; Water Resources SC Environmental Sciences & Ecology; Marine & Freshwater Biology; Water Resources GA 281WM UT WOS:000254529600004 ER PT J AU Eriksen, HK Jewell, JB Dickinson, C Banday, AJ Gorski, KM Lawrence, CR AF Eriksen, H. K. Jewell, J. B. Dickinson, C. Banday, A. J. Gorski, K. M. Lawrence, C. R. TI Joint Bayesian component separation and CMB power spectrum estimation SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmic microwave background; cosmology : observations; methods : numerical ID MICROWAVE BACKGROUND ANISOTROPY; PROBE WMAP OBSERVATIONS; SKY MAPS; FOREGROUNDS; POLARIZATION; TEMPERATURE; RADIATION; TEMPLATE; EMISSION; FASTICA AB We describe and implement an exact, flexible, and computationally efficient algorithm for joint component separation and CMB power spectrum estimation, building on a Gibbs sampling framework. Two essential new features are ( 1) conditional sampling of foreground spectral parameters and ( 2) joint sampling of all amplitude-type degrees of freedom ( e. g., CMB, foreground pixel amplitudes, and global template amplitudes) given spectral parameters. Given a parametric model of the foreground signals, we estimate efficiently and accurately the exact joint foreground-CMB posterior distribution and, therefore, all marginal distributions such as the CMB power spectrum or foreground spectral index posteriors. The main limitation of the current implementation is the requirement of identical beam responses at all frequencies, which restricts the analysis to the lowest resolution of a given experiment. We outline a future generalization to multiresolution observations. To verify the method, we analyze simple models and compare the results to analytical predictions. We then analyze a realistic simulation with properties similar to the 3 yr WMAP data, downgraded to a common resolution of 3 degrees FWHM. The results from the actual 3 yr WMAP temperature analysis are presented in a companion Letter. C1 [Eriksen, H. K.] Univ Oslo, Inst Theoret Astrophys, N-0315 Oslo, Norway. [Eriksen, H. K.] Univ Oslo, Ctr Math Appl, N-0316 Oslo, Norway. [Jewell, J. B.; Dickinson, C.; Gorski, K. M.; Lawrence, C. R.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Banday, A. J.] Max Planck Inst Astrophys, D-85741 Munich, Germany. [Gorski, K. M.] Warsaw Univ Observat, PL-00478 Warsaw, Poland. RP Eriksen, HK (reprint author), Univ Oslo, Inst Theoret Astrophys, POB 1029 Blindern, N-0315 Oslo, Norway. EM h.k.k.eriksen@astro.uio.no NR 30 TC 85 Z9 86 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAR 20 PY 2008 VL 676 IS 1 BP 10 EP 32 DI 10.1086/525277 PG 23 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 275QG UT WOS:000254086100002 ER PT J AU Assef, RJ Kochanek, CS Brodwin, M Brown, MJI Caldwell, N Cool, RJ Eisenhardt, P Eisenstein, D Gonzalez, AH Jannuzi, BT Jones, C McKenzie, E Murray, SS Stern, D AF Assef, R. J. Kochanek, C. S. Brodwin, M. Brown, M. J. I. Caldwell, N. Cool, R. J. Eisenhardt, P. Eisenstein, D. Gonzalez, A. H. Jannuzi, B. T. Jones, C. McKenzie, E. Murray, S. S. Stern, D. TI Low-resolution spectral templates for galaxies from 0.2 to 10 mu m SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : distances and redshifts; galaxies : luminosity function, mass function; galaxies : photometry ID DIGITAL SKY SURVEY; INFRARED ARRAY CAMERA; SPITZER-SPACE-TELESCOPE; BROAD-BAND PHOTOMETRY; STAR-FORMING GALAXIES; LYMAN BREAK GALAXIES; IRAC SHALLOW SURVEY; WIDE-FIELD SURVEY; LUMINOSITY FUNCTION; ENERGY-DISTRIBUTIONS AB We built an optimal basis of low- resolution templates for galaxies over the wavelength range from 0.2 to 10 mu m using a variant of the algorithm presented by Budavari and coworkers. We derived them using 11 bands of photometry from the NDWFS, FLAMEX, zBootes, and IRAC Shallow surveys for 16,033 galaxies in the NDWFS Bootes field with spectroscopic redshifts measured by the AGN and Galaxy Evolution Survey. We also developed algorithms to accurately determine photometric redshifts, K-corrections, and bolometric luminosities using these templates. Our photometric redshifts have an accuracy of sigma(z)/(1+z) = 0.04 when clipped to the best 95%. We used these templates to study the spectral type distribution in the field and to estimate luminosity functions of galaxies as a function of redshift and spectral type. In particular, we note that the 5 - 8 mu m color distribution of galaxies is bimodal, much like the optical g - r colors. C1 [Assef, R. J.; Kochanek, C. S.] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA. [Brodwin, M.; Eisenhardt, P.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Brown, M. J. I.] Monash Univ, Sch Phys, Clayton, Vic 3800, Australia. [Caldwell, N.; Murray, S. S.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Cool, R. J.; Eisenstein, D.] Univ Arizona, Steward Observ, Tucson, AZ 85121 USA. [Gonzalez, A. H.] Univ Florida, Dept Astron, Gainesville, FL 32611 USA. [Jannuzi, B. T.] Kitt Peak Natl Observ, Natl Opt Astron Observ, Tucson, AZ 85726 USA. [McKenzie, E.] Colgate Univ, Dept Phys & Astron, Hamilton, NY 13346 USA. RP Assef, RJ (reprint author), Ohio State Univ, Dept Astron, 140 W 18th Ave, Columbus, OH 43210 USA. RI Brown, Michael/B-1181-2015 OI Brown, Michael/0000-0002-1207-9137 NR 63 TC 45 Z9 45 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAR 20 PY 2008 VL 676 IS 1 BP 286 EP 303 DI 10.1086/527533 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 275QG UT WOS:000254086100020 ER PT J AU Beirao, P Brandl, BR Appleton, PN Groves, B Armus, L Schreiber, NMF Smith, JD Charmandaris, V Houck, JR AF Beirao, P. Brandl, B. R. Appleton, P. N. Groves, B. Armus, L. Schreiber, N. M. Foerster Smith, J. D. Charmandaris, V. Houck, J. R. TI Spatially resolved spitzer IRS spectroscopy of the central region of M82 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : individual (M82); galaxies : starburst; infrared : galaxies ID STARBURST GALAXY M82; AROMATIC-HYDROCARBON EMISSION; RESOLUTION X-RAY; INFRARED SPECTROGRAPH; INTERSTELLAR DUST; STAR-FORMATION; MU-M; MIDINFRARED SPECTROSCOPY; MOLECULAR-HYDROGEN; SPACE-TELESCOPE AB We present high spatial resolution ( similar to 35 pc) 5-38 mu m spectra of the central region of M82, taken with the Spitzer Infrared Spectrograph. From these spectra we determined the fluxes and equivalent widths ( EWs) of key diagnostic features, such as the [Ne-II] 12.8 mu m, [Ne-III] 15.5 mu m, and H-2 S(1) 17.03 mu m lines, and the broad mid-IR polycyclic aromatic hydrocarbon (PAH) emission features in six representative regions and analyzed the spatial distribution of these lines and their ratios across the central region. We find a good correlation of the dust extinction with the CO 1-0 emission. The PAH emission follows closely the ionization structure along the galactic disk. The observed variations of the diagnostic PAH ratios across M82 can be explained by extinction effects, within systematic uncertainties. The 16-18 mu m PAH complex is very prominent, and its EW is enhanced outward from the galactic plane. We interpret this as a consequence of the variation of the UV radiation field. The EWs of the 11.3 mu m PAH feature and the H-2 S( 1) line correlate closely, and we conclude that shocks in the outflow regions have no measurable influence on the H-2 emission. The [ Ne-III]/[ Ne-II] ratio is on average low, at similar to 0.18, and shows little variations across the plane, indicating that the dominant stellar population is evolved ( 5-6 Myr) and well distributed. There is a slight increase of the ratio with distance from the galactic plane of M82, which we attribute to a decrease in gas density. Our observations indicate that the star formation rate has decreased significantly in the last 5 Myr. The quantities of dust and molecular gas in the central area of the galaxy argue against starvation and for negative feedback processes, observable through the strong extraplanar outflows. C1 [Beirao, P.; Brandl, B. R.; Groves, B.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. [Appleton, P. N.] CALTECH, NASA, Herschel Sci Ctr, Pasadena, CA 91125 USA. [Armus, L.] CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA. [Schreiber, N. M. Foerster] Max Planck Inst Extraterr Phys, Garching, Germany. [Smith, J. D.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Charmandaris, V.] Fdn Res & Technol Hellas, IESL, GR-71110 Iraklion, Greece. [Houck, J. R.] Cornell Univ, Dept Astron, Ithaca, NY 14853 USA. RP Beirao, P (reprint author), Leiden Univ, Leiden Observ, POB 9513, NL-2300 RA Leiden, Netherlands. RI Charmandaris, Vassilis/A-7196-2008; OI Charmandaris, Vassilis/0000-0002-2688-1956; Appleton, Philip/0000-0002-7607-8766 NR 67 TC 33 Z9 33 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 MAR 20 PY 2008 VL 676 IS 1 BP 304 EP 316 DI 10.1086/527343 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 275QG UT WOS:000254086100021 ER PT J AU Hwang, U Petre, R Flanagan, KA AF Hwang, Una Petre, Robert Flanagan, Kathryn A. TI X-ray-emitting ejecta in Puppis A observed with Suzaku SO ASTROPHYSICAL JOURNAL LA English DT Article DE supernova remnants; X-rays : individual (Puppis A); X-rays : ISM ID CORE-COLLAPSE SUPERNOVAE; LARGE-MAGELLANIC-CLOUD; CYGNUS LOOP; NEUTRAL HYDROGEN; PLASMA STRUCTURE; REMNANT PUPPIS; MASSIVE STARS; RICH EJECTA; NUCLEOSYNTHESIS; SPECTROSCOPY AB We report the detection and localization of X-ray-emitting ejecta in the middle-aged Galactic supernova remnant Puppis A using five observations with the Suzaku X-Ray Imaging Spectrometer to survey the eastern and middle portions of the remnant. Aroughly 3' x 5', double-peaked region in the north center is found to be highly enriched in Si and other elements relative to the rest of the remnant. The X-ray-fitted abundances are otherwise well below the solar values. While the ejecta-enhanced regions show some variation of relative element abundances, there is little evidence for a very strong enhancement of one element over the others in the imaged portion of the remnant, except possibly for a region of O and Ne enhancement in the remnant's south center. There is no general spatial correlation between the compact [OIII]-emitting ejecta knots seen optically and the abundance enhancements seen in X-rays, although they are located in the same vicinity. The map of fitted column density shows strong variations across the remnant that echo earlier X-ray spectral hardness maps. The ionization age (as fitted for single-temperature models) is sharply higher in a ridge behind the northeast-east boundary of the remnant, and is probably related to the strong molecular cloud interaction along that boundary. The temperature map, by comparison, shows relatively weak variations. C1 [Hwang, Una; Petre, Robert] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Hwang, Una] Johns Hopkins Univ, Baltimore, MD 21218 USA. [Flanagan, Kathryn A.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. RP Hwang, U (reprint author), NASA, Goddard Space Flight Ctr, Code 662, Greenbelt, MD 20771 USA. RI XRAY, SUZAKU/A-1808-2009 NR 40 TC 27 Z9 27 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD MAR 20 PY 2008 VL 676 IS 1 BP 378 EP 389 DI 10.1086/528925 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 275QG UT WOS:000254086100027 ER PT J AU Alcala, JM Spezzi, L Chapman, N Evans, NJ Huard, TL Jorgensen, JK Merin, B Stapelfeldt, KR Covino, E Frasca, A Gandolfi, D Oliveira, I AF Alcala, Juan M. Spezzi, Loredana Chapman, Nicholas Evans, Neal J. Huard, Tracy L. Jorgensen, Jes K. Merin, Bruno Stapelfeldt, Karl R. Covino, Elvira Frasca, Antonio Gandolfi, Davide Oliveira, Isa TI The Spitzer c2d survey of large, nearby, interstellar clouds. X. The Chamaeleon II pre-main-sequence population as observed with IRAC and MIPS SO ASTROPHYSICAL JOURNAL LA English DT Review DE circumstellar matter; infrared : stars; planetary systems : protoplanetary disks; stars : formation; stars : low-mass; brown dwarfs; stars : pre-main-sequence ID T-TAURI STARS; SPECTRAL ENERGY-DISTRIBUTIONS; YOUNG STELLAR OBJECTS; HERBIG-HARO OBJECTS; ALL-SKY SURVEY; MASS-LOSS RATES; DARK-CLOUD; MOLECULAR CLOUDS; FORMING REGION; BROWN DWARF AB We discuss the results from the combined IRAC and MIPS c2d Spitzer Legacy survey observations and complementary optical and NIR data of the Chamaeleon II (Cha II) dark cloud. We perform a census of the young population in an area of similar to 1.75 deg(2) and study the spatial distribution and properties of the cloud members and candidate pre-main-sequence (PMS) objects and their circumstellar matter. Our census is complete down to the substellar regime (M approximate to 0.03 M-circle dot). From the analysis of the volume density of the PMS objects and candidates we find two groups of objects with volume densities higher than 25 M-circle dot pc(-3) and 5-10 members each. A multiplicity fraction of about 13% +/- 3% is observed for objects with separations 0.8 '' < theta < 6.0 '' (142-1065 AU). No evidence for variability between the two epochs of the c2d IRAC data set, Delta t similar to 6 hr, is detected. We estimate a star formation efficiency of 1%-4%, consistent with the estimates for Taurus and Lupus, but lower than for Cha I. This might mean that different star formation activities in the Chamaeleon clouds reflect a different history of star formation. We also find that Cha II is turning some 6-7 M-circle dot into stars every Myr, which is low in comparison with the star formation rate in other c2d clouds. The disk fraction of 70%-80% that we estimate in Cha II is much higher than in other star-forming regions and indicates that the population in this cloud is dominated by objects with active accretion. Finally, the Cha II outflows are discussed; a new Herbig-Haro outflow, HH 939, driven by the classical T Tauri star Sz 50, has been discovered. C1 [Alcala, Juan M.; Spezzi, Loredana; Covino, Elvira] Osserv Astron Capodimonte, INAF, I-80131 Naples, Italy. [Spezzi, Loredana; Frasca, Antonio; Gandolfi, Davide] Osserv Astrofis Catania, INAF, I-95123 Catania, Italy. [Chapman, Nicholas] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Evans, Neal J.] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA. [Huard, Tracy L.] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. [Jorgensen, Jes K.] Univ Bonn, Argelander Inst Astron, D-53121 Bonn, Germany. [Merin, Bruno] European Space Agcy, Res & Sci Support Dept ESTEC, NL-2200 AG Noordwijk, Netherlands. [Merin, Bruno; Oliveira, Isa] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. [Stapelfeldt, Karl R.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Oliveira, Isa] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. RP Alcala, JM (reprint author), Osserv Astron Capodimonte, INAF, I-80131 Naples, Italy. EM alcala@oacn.inaf.it; chapman@astro.umd.edu; nje@astro.as.utexas.edu; thuard@cfa.harvard.edu; jes@astro.uni-bonn.de; bmerin@rssd.esa.int; krs@exoplanet.jpl.nasa.gov; afr@oact.inaf.it; isa@gps.caltech.edu RI Stapelfeldt, Karl/D-2721-2012; OI Alcala, Juan Manuel/0000-0001-8657-095X; Frasca, Antonio/0000-0002-0474-0896; Covino, Elvira/0000-0002-6187-6685; Gandolfi, Davide/0000-0001-8627-9628; Merin, Bruno/0000-0002-8555-3012 NR 114 TC 57 Z9 57 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD MAR 20 PY 2008 VL 676 IS 1 BP 427 EP 463 DI 10.1086/527315 PG 37 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 275QG UT WOS:000254086100033 ER PT J AU Roberge, A Weinberger, AJ AF Roberge, Aki Weinberger, Alycia J. TI Debris disks around nearby stars with circumstellar gas SO ASTROPHYSICAL JOURNAL LA English DT Article DE circumstellar matter; infrared : stars; planetary systems : formation; stars : early-type ID A-SHELL STARS; BETA-PICTORIS; DUST; EMISSION; CATALOG; SYSTEM; EXCESS AB We conducted a survey for infrared excess emission from 16 nearby main-sequence shell stars using the Multiband Imaging Photometer for Spitzer (MIPS) on the Spitzer Space Telescope. Shell stars are early-type stars with narrow absorption lines in their spectra that appear to arise from circumstellar (CS) gas. Four of the 16 stars in our survey showed excess emission at 24 and 70 mu m characteristic of cool CS dust and are likely to be edge-on debris disks. Including previously known disks, it appears that the fraction of protoplanetary and debris disks among the main-sequence shell stars is at least 48% +/- 14%. While dust in debris disks has been extensively studied, relatively little is known about their gas content. In the case of beta Pictoris, extensive observations of gaseous species have provided insights into the dynamics of the CS material and surprises about the composition of the CS gas coming from young planetesimals. To understand the coevolution of gas and dust through the terrestrial planet formation phase, we need to study the gas in additional debris disks. The new debris disk candidates from this Spitzer survey double the number of systems in which the gas can be observed right now with sensitive line-of-sight absorption spectroscopy. C1 [Roberge, Aki] NASA, Goddard Space Flight Ctr, Exoplanets & Stellar Astrophys Lab, Greenbelt, MD 20771 USA. [Weinberger, Alycia J.] Carnegie Inst Washington, Dept Terr Magnetism, Washington, DC 20015 USA. RP Roberge, A (reprint author), NASA, Goddard Space Flight Ctr, Exoplanets & Stellar Astrophys Lab, Code 667, Greenbelt, MD 20771 USA. EM Aki.Roberge@nasa.gov; aweinberger@ciw.edu RI Roberge, Aki/D-2782-2012; OI Roberge, Aki/0000-0002-2989-3725; Weinberger, Alycia/0000-0001-6654-7859 NR 30 TC 21 Z9 21 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 MAR 20 PY 2008 VL 676 IS 1 BP 509 EP 517 DI 10.1086/527314 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 275QG UT WOS:000254086100037 ER PT J AU Shkolnik, E Bohlender, DA Walker, GAH Cameron, AC AF Shkolnik, Evgenya Bohlender, David A. Walker, Gordon A. H. Cameron, Andrew Collier TI The on/off nature of star-planet interactions SO ASTROPHYSICAL JOURNAL LA English DT Article DE planetary systems; radiation mechanisms : nonthermal; stars : activity; stars : chromospheres; stars : individual (tau Boo, HD 179949, HD 209458, HD 189733, HD 217107, HD 149143); stars : late-type ID CA-II H; METALLICITY-BIASED SEARCH; EXTRASOLAR GIANT PLANETS; TRANSITING HOT JUPITERS; K-STAR; SPECTROPOLARIMETRIC OBSERVATIONS; CHROMOSPHERIC ACTIVITY; MAGNETIC-FIELD; HOST STARS; TAU-BOOTIS AB Evidence suggesting an observable magnetic interaction between a star and its hot Jupiter appears as a cyclic variation of stellar activity synchronized to the planet's orbit. In this study we monitored the chromospheric activity using several stellar activity indicators of seven stars with hot Jupiters using new high-resolution echelle spectra collected with ESPaDOnS over a few nights in 2005 and 2006 from the CFHT (Ca II H lambda 3968, K lambda 3933, the Ca II infrared triplet [IRT] lambda 8662 line, H alpha lambda 6563, and He I lambda 5876). Synchronicity of the Ca II H and K emission of HD 179949 with its planet's orbit is clearly seen in four out of six epochs, while rotational modulation with P(rot) = 7 days is apparent in the other two seasons. We observe a similar phenomenon on upsilon And. This on/off nature of star-planet interaction (SPI) in the two systems is likely a function of the changing stellar magnetic field structure throughout its activity cycle. Variability in the transiting system HD 189733 is likely associated with an active region rotating with the star; however, the flaring in excess of the rotational modulation may be associated with its hot Jupiter. As for HD 179949, the peak variability as measured by the mean absolute deviation ( MAD) for both HD 189733 and tau Boo leads the subplanetary longitude by similar to 70 degrees. The tentative correlation between this activity and the ratio of M(p) sin i to the planet's rotation period, a quantity proportional to the hot Jupiter's magnetic moment, first presented by Shkolnik and coworkers remains viable. This work furthers the characterization of SPI, improving its potential as a probe of extrasolar planetary magnetic fields. C1 [Shkolnik, Evgenya] Univ Hawaii Manoa, Inst Astron, NASA Astrobiol Inst, Honolulu, HI 96822 USA. [Bohlender, David A.] Natl Res Council Canada, Herzberg Inst Astrophys, Victoria, BC V9E 2E7, Canada. [Cameron, Andrew Collier] Univ St Andrews, Sch Phys & Astron, St Andrews KY16 9SS, Fife, Scotland. RP Shkolnik, E (reprint author), Univ Hawaii Manoa, Inst Astron, NASA Astrobiol Inst, Honolulu, HI 96822 USA. EM shkolnik@ifa.hawaii.edu; david.bohlender@nrc-cnrc.gc.ca; gordonwa@uvic.ca; acc4@st-andrews.ac.uk OI Cameron, Andrew/0000-0002-8863-7828 NR 51 TC 113 Z9 113 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAR 20 PY 2008 VL 676 IS 1 BP 628 EP 638 DI 10.1086/527351 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 275QG UT WOS:000254086100047 ER PT J AU Winebarger, AR Warren, HP Falconer, DA AF Winebarger, Amy R. Warren, Harry P. Falconer, David A. TI Modeling X-ray loops and EUV "moss" in an active region core SO ASTROPHYSICAL JOURNAL LA English DT Article DE sun : corona ID TRANSITION-REGION; CORONAL-EXPLORER; MAGNETIC-FIELD; TRACE; TEMPERATURE; TELESCOPE; EMISSION; DYNAMICS AB The soft X-ray intensity of loops in active region cores and the corresponding footpoint, or moss, intensity observed in the EUV remain steady for several hours of observation. The steadiness of the emission has prompted many to suggest that the heating in these loops must also be steady, although no direct comparison between the observed X-ray and EUV intensities and the steady heating solutions of the hydrodynamic equations has yet been made. In this paper we perform these simulations and simultaneously model the X-ray and EUV moss intensities in one active region core with steady uniform heating. To perform this task, we introduce a new technique to constrain the model parameters using the measured EUV footpoint intensity to infer a heating rate. Using an ensemble of loop structures derived from magnetic field extrapolation of photospheric field, we associate each field line with an EUV moss intensity, then determine the steady uniform heating rate on that field line that reproduces the observed EUV intensity within 5% for a specific cross-sectional area, or filling factor. We then calculate the total X-ray filter intensities from all loops in the ensemble and compare this to the observed X-ray intensities. We complete this task iteratively to determine the filling factor that returns the best match to the observed X-ray intensities. We find that a filling factor of 8% and loops that expand with height provides the best agreement with the intensity in two X-ray filters, although the simulated SXT Al12 intensity is 147% the observed intensity and the SXT AlMg intensity is 80% the observed intensity. From this solution we determine the required heating rate scales as (B) over bar L-0.29(-0:95). Finally, we discuss the future potential of this type of modeling, such as the ability to use density measurements to fully constrain filling factor, and its shortcomings, such as the requirement to use potential field extrapolations to approximate the coronal field. C1 [Winebarger, Amy R.] Alabama A&M Univ, Normal, AL 35762 USA. [Warren, Harry P.] USN, Res Lab, Washington, DC 20375 USA. [Falconer, David A.] NASA, George C Marshall Space Flight Ctr, Dept Space Sci, Huntsville, AL 35812 USA. RP Winebarger, AR (reprint author), Alabama A&M Univ, 4900 Meridian St,POB 1268, Normal, AL 35762 USA. EM winebarger@physics.aamu.edu; hwarren@nrl.navy.mil; david.falconer@msfc.nasa.gov NR 28 TC 23 Z9 24 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD MAR 20 PY 2008 VL 676 IS 1 BP 672 EP 679 DI 10.1086/527291 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 275QG UT WOS:000254086100051 ER PT J AU Liu, W Petrosian, V Dennis, BR Jiang, YW AF Liu, Wei Petrosian, Vahe Dennis, Brian R. Jiang, Yan Wei TI Double coronal hard and soft X-ray source observed by RHESSI: Evidence for magnetic reconnection and particle acceleration in solar flares SO ASTROPHYSICAL JOURNAL LA English DT Article DE acceleration of particles; Sun : corona; Sun : flares; Sun : X-rays, gamma rays ID STOCHASTIC ACCELERATION; ELECTRON ACCELERATION; ATOMIC DATABASE; EMISSION-LINES; LOOP; SPECTRA; BURSTS; ENERGY; CHIANTI; EVENTS AB We present data analysis and interpretation of an M1.4 class flare observed with the Reuven Ramaty High Energy Solar Spectroscopic Imager (RHESSI) on 2002 April 30. This event, with its footpoints occulted by the solar limb, exhibits a rarely observed, but theoretically expected, double-source structure in the corona. The two coronal sources, observed over the 6-30 keV range, appear at different altitudes and show energy-dependent structures with the higher energy emission being closer together. Spectral analysis implies that the emission at higher energies in the inner region between the two sources is mainly nonthermal, while the emission at lower energies in the outer region is primarily thermal. The two sources are both visible for about 12 minutes and have similar light curves and power-law spectra above about 20 keV. These observations suggest that the magnetic reconnection site lies between the two sources. Bidirectional outflows of the released energy in the form of turbulence and/or particles from the reconnection site could be the source of the observed radiation. The spatially resolved thermal emission below about 15 keV, on the other hand, indicates that the lower source has a larger emission measure but a lower temperature than the upper source. This is likely the result of the differences in the magnetic field and plasma density of the two sources. C1 [Liu, Wei; Dennis, Brian R.] NASA, Goddard Space Flight Ctr, Heliophys Sci Div, Greenbelt, MD 20771 USA. [Liu, Wei; Petrosian, Vahe; Jiang, Yan Wei] Stanford Univ, Dept Phys, Ctr Space Sci & Astrophys, Stanford, CA 94305 USA. RP Liu, W (reprint author), NASA, Goddard Space Flight Ctr, Heliophys Sci Div, Code 671, Greenbelt, MD 20771 USA. EM weiliu@helio.gsfc.nasa.gov RI Dennis, Brian/C-9511-2012 NR 50 TC 63 Z9 64 U1 0 U2 1 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 MAR 20 PY 2008 VL 676 IS 1 BP 704 EP 716 DI 10.1086/527538 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 275QG UT WOS:000254086100054 ER PT J AU Chandra, D Sharma, A Chellappa, R Cathey, WN Lynch, FE Bowman, RC Wermer, JR Paglieri, SN AF Chandra, Dhanesh Sharma, Archana Chellappa, Raja Cathey, William N. Lynch, Franklin E. Bowman, Robert C., Jr. Wermer, Joseph R. Paglieri, Stephen N. TI Hydriding and structural characteristics of thermally cycled and cold-worked V-0.5 at.%C alloy SO JOURNAL OF ALLOYS AND COMPOUNDS LA English DT Article DE metal hydrides; domain structure; thermal cycling; cold-working; V-0.5 at.%C alloy ID METAL-HYDROGEN SYSTEMS; X-RAY-DIFFRACTION; INTERMETALLIC COMPOUND; H SYSTEMS; HYSTERESIS; VANADIUM; THERMODYNAMICS; ABSORPTION; PRESSURE; NIOBIUM AB High pressure hydrides Of V0.995C0.005 were thermally cycled between beta(2)- and gamma-phases hydrides for potential use in cryocoolers/heat pumps for space applications. The effect of addition of carbon to vanadium, on the plateau enthalpies of the high pressure beta(2) + gamma region is minimal. This is in contrast to the calculated plateau enthalpies for low pressure (a + 01) mixed phases which showed a noticeable lowering of the values. Thermal cycling between beta(2)-and gamma-phase hydrides increased the absorption pressures but desorption pressure did not change significantly and the free energy loss due to hysteresis also increased. Hydriding of the alloy with prior cold-work increased the pressure hysteresis significantly and lowered the hydrogen capacity. In contrast to the alloy without any prior straining (as-cast), desorption pressure of the alloy with prior cold-work also decreased significantly. Microstrains, (1/2), in the beta(2)-phase lattice of the thermally cycled hydrides decreased after 778 cycles and the domain sizes increased. However, in the gamma-phase, both the microstrains and the domain sizes decreased after thermal cycling indicating no particle size effect. The dehydrogenated alpha-phase after 778 thermal cycles also showed residual microstrains. in the lattice, similar to those observed in intermetallic hydrides. The effect of thermal cycling (up to 4000 cycles between beta(2)- and gamma-phases) and cold working on absorption/desorption pressures, hydrogen storage capacity, microstrains, long-range strains, and domain sizes of beta(2)- and gamma-phase hydrides Of V0.995C0.005 alloys are presented. Published by Elsevier B.V. C1 [Chandra, Dhanesh; Sharma, Archana; Chellappa, Raja; Cathey, William N.] Univ Nevada, Reno, NV 89557 USA. [Lynch, Franklin E.] HCI, Littleton, CO 80125 USA. [Bowman, Robert C., Jr.] NASA, Jet Propuls Lab, Pasadena, CA 91109 USA. [Wermer, Joseph R.; Paglieri, Stephen N.] Los Alamos Natl Lab, Los Alamos, NM 87545 USA. RP Chandra, D (reprint author), Univ Nevada, Reno, NV 89557 USA. EM dchandra@unr.edu OI Bowman, Robert/0000-0002-2114-1713 NR 66 TC 21 Z9 21 U1 1 U2 5 PU ELSEVIER SCIENCE SA PI LAUSANNE PA PO BOX 564, 1001 LAUSANNE, SWITZERLAND SN 0925-8388 J9 J ALLOY COMPD JI J. Alloy. Compd. PD MAR 20 PY 2008 VL 452 IS 2 BP 312 EP 324 DI 10.1016/j.jallcom.2006.11.078 PG 13 WC Chemistry, Physical; Materials Science, Multidisciplinary; Metallurgy & Metallurgical Engineering SC Chemistry; Materials Science; Metallurgy & Metallurgical Engineering GA 275UI UT WOS:000254096800024 ER PT J AU Swain, MR Vasisht, G Tinetti, G AF Swain, Mark R. Vasisht, Gautam Tinetti, Giovanna TI The presence of methane in the atmosphere of an extrasolar planet SO NATURE LA English DT Article ID GIANT PLANETS; TRANSMISSION SPECTRA; LIGHT CURVES; WATER-VAPOR; HD 189733B; HD-189733; DYNAMICS; 209458B; TRANSIT; SYSTEM AB Molecules present in the atmospheres of extrasolar planets are expected to influence strongly the balance of atmospheric radiation, to trace dynamical and chemical processes, and to indicate the presence of disequilibrium effects. As molecules have the potential to reveal atmospheric conditions and chemistry, searching for them is a high priority. The rotational - vibrational transition bands of water, carbon monoxide and methane are anticipated to be the primary sources of non- continuum opacity in hot- Jupiter planets(1-3). As these bands can overlap in wavelength, and the corresponding signatures from them are weak, decisive identification requires precision infrared spectroscopy. Here we report a near- infrared transmission spectrum of the planet HD 189733b that shows the presence of methane. Additionally, a resolved water vapour band at 1.9 mu m confirms the recent claim(4) of water in this object. On thermochemical grounds, carbon monoxide is expected to be abundant in the upper atmosphere of hot- Jupiter planets, but is not identifiable here; therefore the detection of methane rather than carbon monoxide in such a hot planet(5,6) could signal the presence of a horizontal chemical gradient away from the permanent dayside, or it may imply an ill- understood photochemical mechanism that leads to an enhancement of methane. C1 [Swain, Mark R.; Vasisht, Gautam] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Tinetti, Giovanna] UCL, Dept Phys & Astron, London WC1E 6BT, England. RP Swain, MR (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM Mark.R.Swain@jpl.nasa.gov OI Tinetti, Giovanna/0000-0001-6058-6654 NR 25 TC 321 Z9 324 U1 5 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 MAR 20 PY 2008 VL 452 IS 7185 BP 329 EP 331 DI 10.1038/nature06823 PG 3 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 276BX UT WOS:000254117400041 PM 18354477 ER PT J AU Uno, I Yumimoto, K Shimizu, A Hara, Y Sugimoto, N Wang, Z Liu, Z Winker, DM AF Uno, I. Yumimoto, K. Shimizu, A. Hara, Y. Sugimoto, N. Wang, Z. Liu, Z. Winker, D. M. TI 3D structure of Asian dust transport revealed by CALIPSO lidar and a 4DVAR dust model SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article AB We present detailed 3D structure of Asian dust outflow from a dust source region to the northwestern Pacific ocean retrieved by NASA/CALIOP onboard CALIPSO and results simulated by a four-dimensional variational (4DVAR) data assimilation version of a dust transport model (RC4) based on the NIES Lidar network. The modeled and CALIOP dust extinction showed good agreement, both for horizontal scale (600-1200 km) and vertical depth (1600-3600 m) near the dust source regions. Cross-section analyses of CALIOP and RC4 assisted by forward trajectory revealed that dust from the Gobi Desert on 5 May traveled approximately 1000-1500 km/day to the east and passed over Japan on 8 May. The elevated dust subsequently passed to the Pacific Ocean while maintaining the major dust layer height of 2500-4000 m MSL trapped within the potential temperature of 302-306 K. Results of our analyses demonstrate the importance of integration of CALIOP measurement and the dust model for clarifying the overall structure of an Asian dust event. C1 Kyushu Univ, Res Inst Appl Mech, Fukuoka 812, Japan. [Yumimoto, K.] Kyushu Univ, Dept Earth Syst Sci & Technol, Fukuoka 812, Japan. [Shimizu, A.; Hara, Y.; Sugimoto, N.] Natl Inst Environm Study, Tsukuba, Ibaraki 3058506, Japan. [Liu, Z.] Natl Inst Atmosphere, Hampton, VA 23666 USA. [Wang, Z.] Chinese Acad Sci, Inst Atmospher Phys, Beijing 100029, Peoples R China. [Winker, D. M.] NASA, Langley Res Ctr, Hampton, VA 23681 USA. [Yumimoto, K.] Kyushu Univ, Dept Earth Syst Sci & Technol, Fukuoka 8168580, Japan. RP Uno, I (reprint author), Kyushu Univ, Res Inst Appl Mech, Fukuoka 812, Japan. EM uno@riam.kyushu-u.ac.jp RI Wang, Zifa/B-5192-2008; Kyushu, RIAM/F-4018-2015; U-ID, Kyushu/C-5291-2016; Liu, Zhaoyan/A-9604-2009; Shimizu, Atsushi/C-2810-2009; Liu, Zhaoyan/B-1783-2010; Uno, Itsushi/B-5952-2011; Wang, ZF/D-7202-2012; Wang, Zifa/B-5799-2011; Yumimoto, Keiya/G-1345-2012; Sugimoto, Nobuo/C-5189-2015 OI Shimizu, Atsushi/0000-0002-7306-7412; Liu, Zhaoyan/0000-0003-4996-5738; Wang, ZF/0000-0002-7062-6012; Yumimoto, Keiya/0000-0002-3465-0613; Sugimoto, Nobuo/0000-0002-0545-1316 NR 9 TC 51 Z9 51 U1 2 U2 8 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD MAR 19 PY 2008 VL 35 IS 6 AR L06803 DI 10.1029/2007GL032329 PG 7 WC Geosciences, Multidisciplinary SC Geology GA 281TC UT WOS:000254520800001 ER PT J AU Wu, SL Mickley, LJ Leibensperger, EM Jacob, DJ Rind, D Streets, DG AF Wu, Shiliang Mickley, Loretta J. Leibensperger, Eric M. Jacob, Daniel J. Rind, David Streets, David G. TI Effects of 2000-2050 global change on ozone air quality in the United States SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID TROPICAL TROPOSPHERIC OZONE; SURFACE OZONE; CLIMATE-CHANGE; ISOPRENE EMISSION; GODDARD-INSTITUTE; MODEL; POLLUTION; DISTRIBUTIONS; SENSITIVITY; CHEMISTRY AB We investigate the effects on U. S. ozone air quality from 2000 - 2050 global changes in climate and anthropogenic emissions of ozone precursors by using a global chemical transport model ( GEOS- Chem) driven by meteorological fields from the NASA Goddard Institute for Space Studies general circulation model ( NASA/ GISS GCM). We follow the Intergovernmental Panel on Climate Change A1B scenario and separate the effects from changes in climate and anthropogenic emissions through sensitivity simulations. The 2000 - 2050 changes in anthropogenic emissions reduce the U. S. summer daily maximum 8- hour ozone by 2 - 15 ppb, but climate change causes a 2 - 5 ppb positive offset over the Midwest and northeastern United States, partly driven by decreased ventilation from convection and frontal passages. Ozone pollution episodes are far more affected by climate change than mean values, with effects exceeding 10 ppb in the Midwest and northeast. We find that ozone air quality in the southeast is insensitive to climate change, reflecting compensating effects from changes in isoprene emission and air pollution meteorology. We define a " climate change penalty'' as the additional emission controls necessary to meet a given ozone air quality target. We find that a 50% reduction in U. S. NOx emissions is needed in the 2050 climate to reach the same target in the Midwest as a 40% reduction in the 2000 climate. Emission controls reduce the magnitude of this climate change penalty and can even turn it into a climate benefit in some regions. C1 [Wu, Shiliang; Mickley, Loretta J.; Leibensperger, Eric M.; Jacob, Daniel J.] Harvard Univ, Sch Engn & Appl Sci, Cambridge, MA 02138 USA. [Rind, David] NASA, Goddard Inst Space Studies, New York, NY 10025 USA. [Streets, David G.] Argonne Natl Lab, Argonne, IL 60439 USA. RP Wu, SL (reprint author), Harvard Univ, Sch Engn & Appl Sci, Pierce Hall,20 Oxford St, Cambridge, MA 02138 USA. EM s.wu@post.harvard.edu RI Mickley, Loretta/D-2021-2012; Chem, GEOS/C-5595-2014; OI Mickley, Loretta/0000-0002-7859-3470; Streets, David/0000-0002-0223-1350 NR 64 TC 126 Z9 127 U1 2 U2 34 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 MAR 19 PY 2008 VL 113 IS D6 AR D06302 DI 10.1029/2007JD008917 PG 12 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 281UC UT WOS:000254523400002 ER PT J AU Stockli, R Lawrence, DM Niu, GY Oleson, KW Thornton, PE Yang, ZL Bonan, GB Denning, AS Running, SW AF Stoeckli, R. Lawrence, D. M. Niu, G. -Y. Oleson, K. W. Thornton, P. E. Yang, Z. -L. Bonan, G. B. Denning, A. S. Running, S. W. TI Use of FLUXNET in the community land model development SO JOURNAL OF GEOPHYSICAL RESEARCH-BIOGEOSCIENCES LA English DT Article ID SURFACE PARAMETRIZATION SCHEMES; ATMOSPHERE COUPLING EXPERIMENT; CARBON-DIOXIDE EXCHANGE; ENERGY-BALANCE CLOSURE; MIXED HARDWOOD FOREST; CLIMATE SYSTEM MODEL; INTERANNUAL VARIATION; SPRUCE FOREST; GLOBAL-MODELS; WATER AB The Community Land Model version 3 (CLM3.0) simulates land-atmosphere exchanges in response to climatic forcings. CLM3.0 has known biases in the surface energy partitioning as a result of deficiencies in its hydrological and biophysical parameterizations. Such models, however, need to be robust for multidecadal global climate simulations. FLUXNET now provides an extensive data source of carbon, water and energy exchanges for investigating land processes, and it encompasses a global range of ecosystem-climate interactions. Data from 15 FLUXNET sites are used to identify and improve model deficiencies. Including a prognostic aquifer, a bare soil evaporation resistance formulation and numerous other changes in the model result in a significantly improved soil hydrology and energy partitioning. Terrestrial water storage increased by up to 300 mm in warm climates and decreased in cold climates. Nitrogen control of photosynthesis is revealed as another missing process in the model. These improvements increase the correlation coefficient of hourly and monthly latent heat fluxes from a range of 0.5-0.6 to the range of 0.7-0.9. RMSE of the simulated sensible heat fluxes decrease by 20-50%. Primary production is overestimated during the wet season in mediterranean and tropical ecosystems. This might be related to missing carbon-nitrogen dynamics as well as to site-specific parameters. The new model (CLM3.5) with an improved terrestrial water cycle should lead to more realistic land-atmosphere exchanges in coupled simulations. FLUXNET is found to be a valuable tool to develop and validate land surface models prior to their application in computationally expensive global simulations. C1 [Stoeckli, R.; Denning, A. S.] Colorado State Univ, Dept Atmospher Sci, Ft Collins, CO 80523 USA. [Stoeckli, R.] MeteoSwiss, Climate Serv, Fed Off Meteorol & Climatol, CH-8044 Zurich, Switzerland. [Stoeckli, R.] NASA, Goddard Space Flight Ctr, Earth Observ, Greenbelt, MD 20771 USA. [Lawrence, D. M.; Oleson, K. W.; Thornton, P. E.; Bonan, G. B.] Natl Ctr Atmospher Res, Terr Sci Sect, Boulder, CO 80305 USA. [Niu, G. -Y.; Yang, Z. -L.] Univ Texas Austin, Dept Geol Sci, Austin, TX 78712 USA. [Running, S. W.] Univ Montana, Numer Terradynam Simulat Grp, Missoula, MT 59812 USA. RP Stockli, R (reprint author), Colorado State Univ, Dept Atmospher Sci, Ft Collins, CO 80523 USA. EM reto.stoeckli@meteoswiss.ch RI Oleson, Keith/A-9328-2008; Lawrence, David/C-4026-2011; Yang, Zong-Liang/B-4916-2011; Thornton, Peter/B-9145-2012; Denning, Scott/F-4974-2011; Niu, Guo-Yue/B-8317-2011; Vuichard, Nicolas/A-6629-2011 OI Lawrence, David/0000-0002-2968-3023; Thornton, Peter/0000-0002-4759-5158; Denning, Scott/0000-0003-3032-7875; NR 84 TC 127 Z9 130 U1 5 U2 45 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-8953 J9 J GEOPHYS RES-BIOGEO JI J. Geophys. Res.-Biogeosci. PD MAR 19 PY 2008 VL 113 IS G1 AR G01025 DI 10.1029/2007JG000562 PG 19 WC Environmental Sciences; Geosciences, Multidisciplinary SC Environmental Sciences & Ecology; Geology GA 281UE UT WOS:000254523600001 ER PT J AU Khazanov, GV Tel'nikhin, AA Kronberg, TK AF Khazanov, G. V. Tel'nikhin, A. A. Kronberg, T. K. TI Dynamic theory of relativistic electrons stochastic heating by whistler mode waves with application to the Earth magnetosphere SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article ID CHAOTIC MOTION; ACCELERATION; PARTICLE; FIELD; SCATTERING; PACKET AB In the Hamiltonian approach, electron motion in a coherent packet of the whistler mode waves propagating along the direction of an ambient magnetic field is studied. The physical processes by which these particles are accelerated to high energy are established. Equations governing particle motion are transformed into a closed pair of nonlinear difference equations. The solutions of these equations show there exists a threshold in initial electron energy, below which electron motion is regular and above which electron motion is stochastic. Particle energy spectra and pitch angle electron scattering are described by the Fokker-Planck-Kolmogorov equations. A calculation of the stochastic diffusion of electrons due to a spectrum of whistler modes is presented. The parametric dependence of the diffusion coefficients on the plasma particle density, magnitude of wave field, and the strength of magnetic field is studied. It is shown that significant pitch angle diffusion occurs for the Earth radiation belt electrons with energies from a few keV up to a few MeV. C1 [Khazanov, G. V.] NASA, George C Marshall Space Flight Ctr, Natl Space Sci & Technol Ctr, Huntsville, AL 35805 USA. [Tel'nikhin, A. A.; Kronberg, T. K.] Altai State Univ, Dept Phys, Barnaul 656049, Russia. RP Khazanov, GV (reprint author), NASA, George C Marshall Space Flight Ctr, Natl Space Sci & Technol Ctr, 320 Sparkman Dr, Huntsville, AL 35805 USA. EM george.khazanov@nsstc.nasa.gov; tatiana.kronberg@list.ru NR 26 TC 8 Z9 8 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 MAR 19 PY 2008 VL 113 IS A3 AR A03207 DI 10.1029/2007JA012488 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 281VM UT WOS:000254527000001 ER PT J AU Grefenstette, BW Smith, DM Dwyer, JR Fishman, GJ AF Grefenstette, B. W. Smith, D. M. Dwyer, J. R. Fishman, G. J. TI Time evolution of terrestrial gamma ray flashes SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article AB We present a study of the time evolution of TGFs observed by both RHESSI and BATSE and compare the data with Monte Carlo simulations of relativistic runaway electron avalanches that record the time of flight for individual photons. Our analysis of the RHESSI data shows that the average delay between the main, hard peak and the secondary, soft tail in the RHESSI data is 28 +/- 3 mu s. We show that this is consistent with Compton downscattering of hard photons in the atmosphere in our simulations when the source region is located at or below 21 km, which is consistent with previous spectroscopic analysis of the RHESSI data. We also show that the much longer delays (nominally 100 mu s) reported for the BATSE TGFs can be understood by the same simulations that are consistent with the RHESSI data once the effects of instrumental deadtime are considered. C1 [Grefenstette, B. W.; Smith, D. M.] Univ Calif Santa Cruz, Santa Cruz Inst Particle Phys, Santa Cruz, CA 95064 USA. [Dwyer, J. R.] Florida Inst Technol, Dept Space Sci, Melbourne, FL 32901 USA. [Fishman, G. J.] NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA. RP Grefenstette, BW (reprint author), Univ Calif Santa Cruz, Santa Cruz Inst Particle Phys, 1156 High St, Santa Cruz, CA 95064 USA. EM bwgref@scipp.ucsc.edu NR 11 TC 41 Z9 42 U1 0 U2 0 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD MAR 18 PY 2008 VL 35 IS 6 AR L06802 DI 10.1029/2007GL032922 PG 5 WC Geosciences, Multidisciplinary SC Geology GA 281TB UT WOS:000254520700004 ER PT J AU Skofronick-Jackson, G Heymsfield, A Holthaus, E Albers, C Kim, MJ AF Skofronick-Jackson, Gail Heymsfield, Andrew Holthaus, Eric Albers, Cerese Kim, Min-Jeong TI Nonspherical and spherical characterization of ice in Hurricane Erin for wideband passive microwave comparisons SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID PART I; MODEL; APPROXIMATION; VERIFICATION; TEMPERATURE; RADIOMETER; PARTICLES; EVOLUTION AB In order to better understand the characteristics and physical-to-radiative relationships of frozen hydrometeors in hurricane systems, computed brightness temperatures (TB) from 10.7 to 183 +/- 10 GHz were compared with radiometric observations of Hurricane Erin (2001) from the NASA ER-2 aircraft. The focus was on the high frequencies (>= 85 GHz) that are particularly sensitive to frozen hydrometeors. In order to initialize the cloud profiles used in the radiative transfer calculations, data from airborne radars, dropsondes, and cloud models were used. Three different ice habit and size parameterizations were used with these cloud profiles to obtain the particle radiative signatures including (1) spherical particles with size distributions derived from in situ observations, (2) spherical "fluffy" snow and graupel particles with modified Marshall-Palmer size distributions, and (3) a non-spherical bullet rosette habit where the radiation attributes (scattering, absorption, and asymmetry properties) were computed using the Discrete Dipole Approximation. In addition, three different reflectivity to ice water content (Z-IWC) relationships were used with the three habit and size parameterizations to provide a measure of the sensitivity of the Z-IWC relationship. This work showed that both the scattering and asymmetry coefficients, along with the ice water content in each layer, play an important role in determining the resultant high frequency brightness temperatures. All low frequency (< 40 GHz) calculations matched the observations with correlation coefficients greater than 0.9. At higher frequencies (> 90 GHz), correlation coefficients ranged from 0.7 to 0.92. Comparing between the three ice habit and size parameterizations showed less than a 0.2 difference in correlation coefficient, while the comparisons between the three Z-IWC relationships caused changes of up to 0.15 in the correlation coefficients, but they had a significant effect on the mean differences between the observations and the calculations. C1 [Skofronick-Jackson, Gail] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Heymsfield, Andrew] Natl Ctr Atmospher Res, Boulder, CO 80307 USA. [Holthaus, Eric] Columbia Univ, New York, NY USA. [Albers, Cerese] Florida State Univ, Tallahassee, FL 32306 USA. [Kim, Min-Jeong] NOAA, Camp Springs, MD USA. RP Skofronick-Jackson, G (reprint author), NASA, Goddard Space Flight Ctr, Code 614-6,Bldg 33,RoomA428, Greenbelt, MD 20771 USA. EM gail.s.jackson@nasa.gov RI Heymsfield, Andrew/E-7340-2011; Skofronick-Jackson, Gail/D-5354-2012 NR 33 TC 8 Z9 8 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 MAR 18 PY 2008 VL 113 IS D6 AR D06201 DI 10.1029/2007JD008866 PG 18 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 281UB UT WOS:000254523300002 ER PT J AU Asner, GP Hughes, RF Vitousek, PM Knapp, DE Kennedy-Bowdoin, T Boardman, J Martin, RE Eastwood, M Green, RO AF Asner, Gregory P. Hughes, R. Flint Vitousek, Peter M. Knapp, David E. Kennedy-Bowdoin, Ty Boardman, Joseph Martin, Roberta E. Eastwood, Michael Green, Robert O. TI Invasive plants transform the three-dimensional structure of rain forests SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF AMERICA LA English DT Article DE biological invasion; Hawaii; imaging spectroscopy; LiDAR; tropical forest ID GINGER HEDYCHIUM-GARDNERIANUM; BIOLOGICAL INVASION; HAWAIIAN FORESTS; GLOBAL CHANGE; ECOSYSTEM; LIGHT; GRASS; GAPS AB Biological invasions contribute to global environmental change, but the dynamics and consequences of most invasions are difficult to assess at regional scales. We deployed an airborne remote sensing system that mapped the location and impacts of five highly invasive plant species across 221,875 ha of Hawaiian ecosystems, identifying four distinct ways that these species transform the three-dimensional (3D) structure of native rain forests. In lowland to montane forests, three invasive tree species replace native midcanopy and understory plants, whereas one understory invader excludes native species at the ground level. A fifth invasive nitrogen-fixing tree, in combination with a midcanopy alien tree, replaces native plants at all canopy levels in lowland forests. We conclude that this diverse array of alien plant species, each representing a different growth form or functional type, is changing the fundamental 3D structure of native Hawaiian rain forests. Our work also demonstrates how an airborne mapping strategy can identify and track the spread of certain invasive plant species, determine ecological consequences of their proliferation, and provide detailed geographic information to conservation and management efforts. C1 [Asner, Gregory P.; Knapp, David E.; Kennedy-Bowdoin, Ty; Martin, Roberta E.] Carnegie Inst Washington, Dept Global Ecol, Stanford, CA 94305 USA. [Hughes, R. Flint] US Forest Serv, Inst Pacific Isl Forestry, Hilo, HI 96720 USA. [Vitousek, Peter M.] Stanford Univ, Dept Biol Sci, Stanford, CA 94305 USA. [Boardman, Joseph] Analyt Imaging & Geophys LLC, Boulder, CO 80303 USA. [Eastwood, Michael; Green, Robert O.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Asner, GP (reprint author), Carnegie Inst Washington, Dept Global Ecol, Stanford, CA 94305 USA. EM gpa@stanford.edu RI Asner, Gregory/G-9268-2013 OI Asner, Gregory/0000-0001-7893-6421 NR 30 TC 110 Z9 112 U1 10 U2 79 PU NATL ACAD SCIENCES PI WASHINGTON PA 2101 CONSTITUTION AVE NW, WASHINGTON, DC 20418 USA SN 0027-8424 J9 P NATL ACAD SCI USA JI Proc. Natl. Acad. Sci. U. S. A. PD MAR 18 PY 2008 VL 105 IS 11 BP 4519 EP 4523 DI 10.1073/pnas.0710811105 PG 5 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 278DH UT WOS:000254263300079 PM 18316720 ER PT J AU Hayes, DJ Cohen, WB Sader, SA Irwin, DE AF Hayes, Daniel J. Cohen, Warren B. Sader, Steven A. Irwin, Daniel E. TI Estimating proportional change in forest cover as a continuous variable from multi-year MODIS data SO REMOTE SENSING OF ENVIRONMENT LA English DT Article DE MODIS; regression models; tropical forests; land cover and land use change ID RESOLUTION IMAGING SPECTRORADIOMETER; NOAA AVHRR DATA; SATELLITE DATA; TROPICAL DEFORESTATION; VEGETATION INDEXES; BIOSPHERE RESERVE; BRAZILIAN AMAZON; LANDSAT; IMAGERY; SCALE AB This article describes a series of fundamental analyses designed to test and compare the utility of various MODIS data and products for detecting land cover change over a large area of the tropics. The approach for estimating proportional forest cover change as a continuous variable was based on a reduced major axis regression model. The model relates multispectral and multi-temporal MODIS data, transformed to optimize the spectral detection of vegetation changes, to reference change data sets derived from a Landsat data record for several study sites across the Central American region. Three MODIS data sets with diverse attributes were evaluated on model consistency, prediction accuracy and practical utility in estimating change in forest cover over multiple time intervals and spatial extents. A spectral index based on short-wave infrared information (normalized difference moisture index), calculated from half-kilometer Calibrated Radiances data sets, generally showed the best relationships with the reference data and the lowest model prediction errors at individual study areas and time intervals. However, spectral indices based on atmospherically corrected surface reflectance data, as with the Vegetation Indices and Nadir Bidirectional Reflectance Distribution Function - Adjusted Reflectance (NBAR) data sets, produced consistent model parameters and accurate forest cover change estimates when modeling over multiple time intervals. Models based on anniversary date acquisitions of the one-kilometer resolution NBAR product proved to be the most consistent and practical to implement. Linear regression models based on spectral indices that correlate with change in the brightness, greenness and wetness spectral domains of these data estimated proportional change in forest cover with less than 10% prediction error over the full spatial and temporal extent of this study. (C) 2007 Elsevier Inc. All rights reserved. C1 [Hayes, Daniel J.] Oregon State Univ, Dept Forest Sci, Corvallis, OR 97331 USA. [Cohen, Warren B.] US Forest Serv, Pacific NW Res Stn, Forestry Sci Lab, Corvallis, OR 97331 USA. [Sader, Steven A.] Univ Maine, Sch Forest Resources, Orono, ME 04469 USA. [Irwin, Daniel E.] NASA, George C Marshall Space Flight Ctr, Global Hydrol & Climate Ctr, Huntsville, AL 35805 USA. RP Hayes, DJ (reprint author), Oregon State Univ, Dept Forest Sci, 321 Richardson Hall, Corvallis, OR 97331 USA. EM Daniel.Hayes@Oregonstate.edu RI Hayes, Daniel/B-8968-2012 NR 48 TC 27 Z9 27 U1 0 U2 8 PU ELSEVIER SCIENCE INC PI NEW YORK PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA SN 0034-4257 J9 REMOTE SENS ENVIRON JI Remote Sens. Environ. PD MAR 18 PY 2008 VL 112 IS 3 BP 735 EP 749 DI 10.1016/j.rse.2007.06.003 PG 15 WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic Technology SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science & Photographic Technology GA 280RK UT WOS:000254443700010 ER PT J AU Del Castillo, CE Miller, RL AF Del Castillo, Carlos E. Miller, Richard L. TI On the use of ocean color remote sensing to measure the transport of dissolved organic carbon by the Mississippi River Plume SO REMOTE SENSING OF ENVIRONMENT LA English DT Article DE CDOM; DOC; SeaWiFS; ocean color; river transport; Mississippi River ID WEST FLORIDA SHELF; BIOOPTICAL PROPERTIES; MATTER; WATERS; CHLOROPHYLL; ABSORPTION; FLUORESCENCE; ALGORITHMS AB We investigated the use of ocean color remote sensing to measure the transport of dissolved organic carbon (DOC) by the Mississippi River to the Gulf of Mexico. From 2000 to 2005 we recorded surface measurements of DOC, colored dissolved organic matter (CDOM), salinity, and water-leaving radiances during five cruises to the Mississippi River Plume. These measurements were used to develop empirical relationships to derive DOC, CDOM, and salinity from monthly composites of SeaWiFS imagery collected from 1998 through 2005. We compared our remote sensing estimates of river flow and DOC transport with data collected by the United States Geological Survey (USGS) from 1998 through 2005. Our remote sensing estimates of river flow and DOC transport correlated well (r(2) similar to 0.70) with the USGS data. Our remote sensing estimates and USGS field data showed low variability in DOC concentrations in the river end-member (7-11%), and high seasonal variability in river flow (similar to 50%). Therefore, changes in river flow control the variability in DOC transport, indicating that the remote sensing estimate of river flow is the most critical element of our DOC transport measurement. We concluded that it is possible to use this method to estimate DOC transport by other large rivers if there are data on the relationship between CDOM, DOC, and salinity in the river plume. (C) 2007 Elsevier Inc. All rights reserved. C1 [Del Castillo, Carlos E.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20707 USA. [Miller, Richard L.] NASA, Stennis Space Ctr, MS USA. RP Del Castillo, CE (reprint author), Johns Hopkins Univ, Appl Phys Lab, Johns Hopkins Rd, Laurel, MD 20707 USA. EM carlos.del.castillo@jhuapl.edu RI Liu, Cheng-Chien/E-4859-2011; Del Castillo, Carlos/N-2601-2013 NR 24 TC 65 Z9 67 U1 3 U2 23 PU ELSEVIER SCIENCE INC PI NEW YORK PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA SN 0034-4257 J9 REMOTE SENS ENVIRON JI Remote Sens. Environ. PD MAR 18 PY 2008 VL 112 IS 3 BP 836 EP 844 DI 10.1016/j.rse.2007.06.015 PG 9 WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic Technology SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science & Photographic Technology GA 280RK UT WOS:000254443700017 ER PT J AU Wulder, MA White, JC Goward, SN Masek, JG Irons, JR Herold, M Cohen, WB Loveland, TR Woodcock, CE AF Wulder, Michael A. White, Joanne C. Goward, Samuel N. Masek, Jeffrey G. Irons, James R. Herold, Martin Cohen, Warren B. Loveland, Thomas R. Woodcock, Curtis E. TI Landsat continuity: Issues and opportunities for land cover monitoring SO REMOTE SENSING OF ENVIRONMENT LA English DT Article DE Landsat; landsat data continuity mission; large area; land cover; monitoring; change detection; remote sensing ID TERM ACQUISITION PLAN; EARTH OBSERVATION; ADVISORY-COMMITTEE; SATELLITE DATA; LARGE AREAS; ASTER; IMAGERY; VALIDATION; MISSION; POLICY AB Initiated in 1972, the Landsat program has provided a continuous record of earth observation for 35 years. The assemblage of Landsat spatial, spectral, and temporal resolutions, over a reasonably sized image extent, results in imagery that can be processed to represent land cover over large areas with an amount of spatial detail that is absolutely unique and indispensable for monitoring, management, and scientific activities. Recent technical problems with the two existing Landsat satellites, and delays in the development and launch of a successor, increase the likelihood that a gap in Landsat continuity may occur. In this communication, we identify the key features of the Landsat program that have resulted in the extensive use of Landsat data for large area land cover mapping and monitoring. We then augment this list of key features by examining the data needs of existing large area land cover monitoring programs. Subsequently, we use this list as a basis for reviewing the current constellation of earth observation satellites to identify potential alternative data sources for large area land cover applications. Notions of a virtual constellation of satellites to meet large area land cover mapping and monitoring needs are also presented. Finally, research priorities that would facilitate the integration of these alternative data sources into existing large area land cover monitoring programs are identified. Continuity of the Landsat program and the measurements provided are critical for scientific, environmental, economic, and social purposes. It is difficult to overstate the importance of Landsat; there are no other systems in orbit, or planned for launch in the short-term, that can duplicate or approach replication, of the measurements and information conferred by Landsat. While technical and political options are being pursued, there is no satellite image data stream poised to enter the National Satellite Land Remote Sensing Data Archive should system failures occur to Landsat-5 and -7. Crown Copyright (C) 2007 Published by Elsevier Inc. All rights reserved. C1 [Wulder, Michael A.; White, Joanne C.] Nat Resources Canada, Pacific Forestry Ctr, Canadian Forest Serv, Victoria, BC V8Z 1M5, Canada. [Goward, Samuel N.] Univ Maryland, Dept Geog, College Pk, MD 20742 USA. [Masek, Jeffrey G.; Irons, James R.] NASA, Goddard Space Flight Ctr, Biospher Sci Branch, Greenbelt, MD 20771 USA. [Herold, Martin] FSU Jena, Dept Geog, GOFC GOLD Land Cover Project Off, Jena, Germany. [Cohen, Warren B.] USDA, Forest Serv, PNW Res Stn, Corvallis, OR 97331 USA. [Loveland, Thomas R.] US Geol Survey, Ctr Earth Observat & Sci EROS, Sioux Falls, SD 57198 USA. [Woodcock, Curtis E.] Boston Univ, Dept Geog, Boston, MA 02215 USA. RP Wulder, MA (reprint author), Nat Resources Canada, Pacific Forestry Ctr, Canadian Forest Serv, 506 W Burnside Rd, Victoria, BC V8Z 1M5, Canada. EM mwulder@nrcan.ge.ca RI Masek, Jeffrey/D-7673-2012; Irons, James/D-8535-2012; Herold, Martin/F-8553-2012; Wulder, Michael/J-5597-2016; OI Herold, Martin/0000-0003-0246-6886; Wulder, Michael/0000-0002-6942-1896; White, Joanne/0000-0003-4674-0373 NR 90 TC 190 Z9 200 U1 12 U2 81 PU ELSEVIER SCIENCE INC PI NEW YORK PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA SN 0034-4257 J9 REMOTE SENS ENVIRON JI Remote Sens. Environ. PD MAR 18 PY 2008 VL 112 IS 3 BP 955 EP 969 DI 10.1016/j.rse.2007.07.004 PG 15 WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic Technology SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science & Photographic Technology GA 280RK UT WOS:000254443700027 ER PT J AU Huang, CQ Song, K Kim, S Townshend, JRG Davis, P Masek, JG Goward, SN AF Huang, Chengquan Song, Kuan Kim, Sunghee Townshend, John R. G. Davis, Paul Masek, Jeffrey G. Goward, Samuel N. TI Use of a dark object concept and support vector machines to automate forest cover change analysis SO REMOTE SENSING OF ENVIRONMENT LA English DT Article DE forest cover change; training data automation; integrated forest index; Landsat; SVM ID REMOTELY-SENSED DATA; ACCURACY ASSESSMENT; LANDSAT DATA; CLASSIFICATION ACCURACY; TROPICAL DEFORESTATION; ATMOSPHERIC CORRECTION; SPATIAL-RESOLUTION; MODIS DATA; REFLECTANCE; ALGORITHM AB An automated method was developed for mapping forest cover change using satellite remote sensing data sets. This multi-temporal classification method consists of a training data automation (TDA) procedure and uses the advanced support vector machines (SVM) algorithm. The TDA procedure automatically generates training data using input satellite images and existing land cover products. The derived high quality training data allow the SVM to produce reliable forest cover change products. This approach was tested in 19 study areas selected from major forest biomes across the globe. In each area a forest cover change map was produced using a pair of Landsat images acquired around 1990 and 2000. High resolution IKONOS images and independently developed reference data sets were available for evaluating the derived change products in 7 of those areas. The overall accuracy values were over 90% for 5 areas, and were 89.4% and 89.6% for the remaining two areas. The user's and producer's accuracies of the forest loss class were over 80% for all 7 study areas, demonstrating that this method is especially effective for mapping major disturbances with low commission errors. IKONOS images were also available in the remaining 12 study areas but they were either located in non-forest areas or in forest areas that did not experience forest cover change between 1990 and 2000. For those areas the IKONOS images were used to assist visual interpretation of the Landsat images in assessing the derived change products. This visual assessment revealed that for most of those areas the derived change products likely were as reliable as those in the 7 areas where accuracy assessment was conducted. The results also suggest that images acquired during leaf-off seasons should not be used in forest cover change analysis in areas where deciduous forests exist. Being highly automatic and with demonstrated capability to produce reliable change products, the TDA-SVM method should be especially usefial for quantifying forest cover change over large areas. (C) 2007 Elsevier Inc. All rights reserved. C1 [Huang, Chengquan; Song, Kuan; Townshend, John R. G.; Davis, Paul; Goward, Samuel N.] Univ Maryland, Dept Geog, College Pk, MD 20742 USA. [Song, Kuan; Kim, Sunghee; Davis, Paul] Univ Maryland, Inst Adv Comp Studies, College Pk, MD 20742 USA. [Masek, Jeffrey G.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Huang, CQ (reprint author), Univ Maryland, Dept Geog, 2181 LeFrak Hall, College Pk, MD 20742 USA. EM cqhuang@umd.edu RI Masek, Jeffrey/D-7673-2012; OI Huang, Chengquan/0000-0003-0055-9798 NR 65 TC 106 Z9 123 U1 7 U2 41 PU ELSEVIER SCIENCE INC PI NEW YORK PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA SN 0034-4257 J9 REMOTE SENS ENVIRON JI Remote Sens. Environ. PD MAR 18 PY 2008 VL 112 IS 3 BP 970 EP 985 DI 10.1016/j.rse.2007.07.023 PG 16 WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic Technology SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science & Photographic Technology GA 280RK UT WOS:000254443700028 ER PT J AU Cho, HM Yang, P Kattawar, GW Nasiri, SL Hu, YX Minnis, P Trepte, C Winker, D AF Cho, Hyoun-Myoung Yang, Ping Kattawar, George W. Nasiri, Shaima L. Hu, Yongxiang Minnis, Patrick Trepte, Charles Winker, David TI Depolarization ratio and attenuated backscatter for nine cloud types: Analyses based on collocated CALIPSO lidar and MODIS measurements SO OPTICS EXPRESS LA English DT Article ID ICE CRYSTALS; WATER-VAPOR; AEROSOL; MISSION AB This paper reports on the relationship between lidar backscatter and the corresponding depolarization ratio for nine types of cloud systems. The data used in this study are the lidar returns measured by the CloudAerosol Lidar with Orthogonal Polarization (CALIOP) aboard the CloudAerosol Lidar and Infrared Pathfinder Satellite Observations (CALIPSO) satellite and the collocated cloud products derived from the observations made by the Moderate Resolution Imaging Spectroradiometer (MODIS) aboard Aqua satellite. Specifically, the operational MODIS cloud optical thickness and cloud-top pressure products are used to classify cloud types on the basis of the International Satellite Cloud Climatology Project (ISCCP) cloud classification scheme. While the CALIPSO observations provide information for up to 10 cloud layers, in the present study only the uppermost clouds are considered. The layer-averaged attenuated backscatter (gamma) and layer-averaged depolarization ratio (delta) from the CALIPSO measurements show both water-and ice-phase features for global cirrus, cirrostratus, and deep convective cloud classes. Furthermore, we screen both the MODIS and CALIPSO data to eliminate cases in which CALIPSO detected two-or multi-layered clouds. It is shown that low gamma values corresponding to uppermost thin clouds are largely eliminated in the CALIPSO delta-gamma relationship for single-layered clouds. For mid-latitude and polar regions corresponding, respectively, to latitude belts 30 degrees-60 degrees and 60 degrees-90 degrees in both the hemispheres, a mixture of water and ice is also observed in the case of the altostratus class. MODIS cloud phase flags are also used to screen ice clouds. The resultant water clouds flagged by the MODIS algorithm show only water phase feature in the delta-gamma relation observed by CALIOP; however, in the case of the ice clouds flagged by the MODIS algorithm, the co-existence of ice-and water-phase clouds is still observed in the CALIPSO delta-gamma relationship. (C)2008 Optical Society of America. C1 [Cho, Hyoun-Myoung; Yang, Ping; Nasiri, Shaima L.] Texas A&M Univ, Dept Atmospher Sci, College Stn, TX 77843 USA. [Kattawar, George W.] Texas A&M Univ, Dept Phys, College Stn, TX 77843 USA. [Hu, Yongxiang; Minnis, Patrick; Trepte, Charles; Winker, David] NASA, Langley Res Ctr, Hampton, VA 23681 USA. RP Yang, P (reprint author), Texas A&M Univ, Dept Atmospher Sci, College Stn, TX 77843 USA. EM pyang@ariel.met.tamu.edu RI Yang, Ping/B-4590-2011; Nasiri, Shaima/C-8044-2011; Hu, Yongxiang/K-4426-2012; Minnis, Patrick/G-1902-2010 OI Minnis, Patrick/0000-0002-4733-6148 NR 29 TC 33 Z9 37 U1 4 U2 16 PU OPTICAL SOC AMER PI WASHINGTON PA 2010 MASSACHUSETTS AVE NW, WASHINGTON, DC 20036 USA SN 1094-4087 J9 OPT EXPRESS JI Opt. Express PD MAR 17 PY 2008 VL 16 IS 6 BP 3931 EP 3948 DI 10.1364/OE.16.003931 PG 18 WC Optics SC Optics GA 276DL UT WOS:000254121400050 PM 18542490 ER PT J AU Savchenkov, AA Rubiola, E Matsko, AB Ilchenko, VS Maleki, L AF Savchenkov, Anatoliy A. Rubiola, Enrico Matsko, Andrey B. Ilchenko, Vladimir S. Maleki, Lute TI Phase noise of whispering gallery photonic hyper-parametric microwave oscillators SO OPTICS EXPRESS LA English DT Article ID OPTOELECTRONIC OSCILLATOR; MODULATIONAL INSTABILITY; FREQUENCY REFERENCES; MODE RESONATORS; FIBER; GENERATION; STABILITY; CAVITY; LASER AB We report on the experimental study of phase noise properties of a high frequency photonic microwave oscillator based on four wave mixing in calcium fluoride whispering gallery mode resonators. Specifically, the oscillator generates similar to 8.5 GHz signals with -120 dBc/Hz at 100 kHz from the carrier. The floor of the phase noise is limited by the shot noise of the signal received at the photodetector. We argue that the performance of the oscillator can be significantly improved if one uses extremely high finesse resonators, increases the input optical power, supersaturates the oscillator, and suppresses the residual stimulated Raman scattering in the resonator. We also disclose a method of extremely sensitive measurement of the integral dispersion of millimeter scale dielectric resonators. (C) 2008 Optical Society of America. C1 [Savchenkov, Anatoliy A.; Rubiola, Enrico; Matsko, Andrey B.; Ilchenko, Vladimir S.; Maleki, Lute] OEwaves Inc, Pasadena, CA 91106 USA. [Rubiola, Enrico; Maleki, Lute] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Rubiola, Enrico] FEMTO ST Inst, CNRS, UMR 6174, Besancon, France. RP Savchenkov, AA (reprint author), OEwaves Inc, 1010 E Union St, Pasadena, CA 91106 USA. EM Andrey.Matsko@oewaves.com NR 29 TC 48 Z9 48 U1 0 U2 14 PU OPTICAL SOC AMER PI WASHINGTON PA 2010 MASSACHUSETTS AVE NW, WASHINGTON, DC 20036 USA SN 1094-4087 J9 OPT EXPRESS JI Opt. Express PD MAR 17 PY 2008 VL 16 IS 6 BP 4130 EP 4144 DI 10.1364/OE.16.004130 PG 15 WC Optics SC Optics GA 276DL UT WOS:000254121400070 PM 18542510 ER PT J AU Kim, H Kim, HI Johnson, PV Beegle, LW Beauchamp, JL Goddard, WA Kanik, I AF Kim, Hyungjun Kim, Hugh I. Johnson, Paul V. Beegle, Luther W. Beauchamp, J. L. Goddard, William A. Kanik, Isik TI Experimental and theoretical investigation into the correlation between mass and ion mobility for choline and other ammonium cations in N-2 SO ANALYTICAL CHEMISTRY LA English DT Article ID ELECTROSPRAY-IONIZATION; GAS-PHASE; AMINO-ACIDS; SPECTROMETRY; SEPARATION; COLLISIONS; BIOMOLECULES; PEPTIDES; ENERGIES; CLUSTERS AB A number of tertiary amine and quaternary ammonium cations spanning a mass range of 60-146 amu (trimethylamine, tetramethylammonium, trimethylethylammonium, N,N-dimethylaminoethanol, choline, N,N-dimethylglycine, betaine, acetylcholine, (3-carboxypropyl)trimethylammonium) were investigated using electrospray ionization ion mobility spectrometry. Measured ion mobilities demonstrate a high correlation between mass and mobility in N-2. In addition, identical mobilities within experimental uncertainties are observed for structurally dissimilar ions with similar ion masses. For example, dimethylethylammonium (88 amu) cations and protonated N,N-dimethylaminoethanol cations (90 amu) show identical mobilities (1.93 cm(2) V-1 s(-1)) though N,N-dimethylaminoethanol contains a hydroxyl functional group while dimethylethylammonium only contains alkyl groups. Computational analysis was performed using the modified trajectory (TJ) method with nonspherical N-2 molecules as the drift gas. The sensitivity of the ammonium cation collision cross sections to the details of the ion-neutral interactions was investigated and compared to other classes of organic molecules (carboxylic acids and abiotic amino acids). The specific charge distribution of the molecular ions in the investigated mass range has an insignificant affect on the collision cross section. C1 [Kim, Hugh I.; Johnson, Paul V.; Beegle, Luther W.; Kanik, Isik] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Kim, Hyungjun; Goddard, William A.] CALTECH, Beckman Inst, Mat & Proc Simulat Ctr, Pasadena, CA 91125 USA. [Kim, Hugh I.; Beauchamp, J. L.] CALTECH, Arthur Amos Noyes Lab Chem Phys, Pasadena, CA 91125 USA. RP Beegle, LW (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM Luther.Beegle@jpl.nasa.gov RI Beegle, Luther/A-6354-2010; Kim, Hugh/G-4476-2011; Kim, Hyungjun/B-4527-2013; Johnson, Paul/D-4001-2009 OI Johnson, Paul/0000-0002-0186-8456 NR 44 TC 28 Z9 28 U1 1 U2 20 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 0003-2700 EI 1520-6882 J9 ANAL CHEM JI Anal. Chem. PD MAR 15 PY 2008 VL 80 IS 6 BP 1928 EP 1936 DI 10.1021/ac701888e PG 9 WC Chemistry, Analytical SC Chemistry GA 274QX UT WOS:000254017000012 PM 18278882 ER PT J AU Sullivan, RM Ghosn, LJ Lerch, BA AF Sullivan, Roy M. Ghosn, Louis J. Lerch, Bradley A. TI A general tetrakaidecahedron model for open-celled foams SO INTERNATIONAL JOURNAL OF SOLIDS AND STRUCTURES LA English DT Article DE foam material; elastic material; energy methods; elongated tetrakaideca hedron; elongated Kelvin model ID ELASTIC PROPERTIES AB A micro-mechanics model for non-isotropic, open-celled foams is developed using an elongated tetrakaidecahedron (Kelvin model) as the repeating unit cell. Assuming the cell edges possess axial and bending rigidity, the mechanics of deformation of the elongated tetrakaidecahedron lead to a set of equations for the Young's modulus, Poisson's ratio and tensile strength of the foam in the principal material directions. These equations are written as a function of the cell edge lengths and cross-section properties, the inclination angle and the strength and stiffness of the solid material. This micro-mechanics model employs an elongated Kelvin model geometry which is more general than that employed by previous authors, as the size and shape of the repeating unit cell are defined by specifying three independent dimensions. As a result, the model accounts for an additional variation in the unit cell shape which is not accounted for in the previous models. The effect of this additional shape parameter on the non-isotropic stiffness and strength behavior is demonstrated and the advantages of this more general micro-mechanics model are illustrated. Published by Elsevier Ltd. C1 [Sullivan, Roy M.; Ghosn, Louis J.; Lerch, Bradley A.] NASA, Glenn Res Ctr, Struct & Mat Div, Cleveland, OH 44135 USA. RP Sullivan, RM (reprint author), NASA, Glenn Res Ctr, Struct & Mat Div, Cleveland, OH 44135 USA. EM roy.sullivan@grc.nasa.gov NR 13 TC 59 Z9 61 U1 2 U2 21 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0020-7683 J9 INT J SOLIDS STRUCT JI Int. J. Solids Struct. PD MAR 15 PY 2008 VL 45 IS 6 BP 1754 EP 1765 DI 10.1016/j.ijsolstr.2007.10.028 PG 12 WC Mechanics SC Mechanics GA 270DO UT WOS:000253700500013 ER PT J AU Killian, JL Zuckerman, NB Niemann, DL Ribaya, BP Rahman, M Espinosa, R Meyyappan, M Nguyen, CV AF Killian, Jessica L. Zuckerman, Nathaniel B. Niemann, Darrell L. Ribaya, Bryan P. Rahman, Mahmud Espinosa, Robert Meyyappan, M. Nguyen, Cattien V. TI Field emission properties of carbon nanotube pillar arrays SO JOURNAL OF APPLIED PHYSICS LA English DT Article ID FILM ELECTRON EMITTERS; MICROSCOPY AB Carbon nanotube pillar arrays (CPAs) for cold field emission applications were grown directly on polished 70/30 at. % NiCr alloy surfaces patterned by photolithography. A carbon nanotube (CNT) pillar is a localized, vertically aligned, and well-ordered group of multiwalled CNTs resulting from van der Waals forces within high-density CNT growth. The edge effect, in which the applied electric field is enhanced along the edge of each pillar, is primarily responsible for the excellent emission properties of CPAs. We achieved efficient emission with turn-on fields as low as 0.9 V/mu m and stable current densities as high as 10 mA/cm(2) at an applied macroscopic field of 5.7 V/mu m. We investigated the effects of pillar aspect ratio, density, and spacing on CPA field emission and quantified the edge effect with respect to pillar aspect ratio through modeling. We also investigated the field emission stability and found substantial improvement with CPAs compared to continuous and patterned CNT films. (c) 2008 American Institute of Physics. C1 [Killian, Jessica L.; Zuckerman, Nathaniel B.; Nguyen, Cattien V.] ELORET Corp, NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Killian, Jessica L.; Zuckerman, Nathaniel B.] San Jose State Univ, Dept Chem, San Jose, CA 95192 USA. [Niemann, Darrell L.; Ribaya, Bryan P.; Rahman, Mahmud] Santa Clara Univ, Electron Devices Lab, Dept Elect Engn, Santa Clara, CA 95053 USA. [Espinosa, Robert] InXitu Inc, Mountain View, CA 94043 USA. RP Nguyen, CV (reprint author), ELORET Corp, NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. EM cvnguyen@mail.arc.nasa.gov NR 28 TC 31 Z9 31 U1 0 U2 14 PU AMER INST PHYSICS PI MELVILLE PA CIRCULATION & FULFILLMENT DIV, 2 HUNTINGTON QUADRANGLE, STE 1 N O 1, MELVILLE, NY 11747-4501 USA SN 0021-8979 J9 J APPL PHYS JI J. Appl. Phys. PD MAR 15 PY 2008 VL 103 IS 6 AR 064312 DI 10.1063/1.2870931 PG 7 WC Physics, Applied SC Physics GA 281ZH UT WOS:000254536900108 ER PT J AU Steinke, IP Ruden, PP Ni, X Morkoc, H Son, KA AF Steinke, I. P. Ruden, P. P. Ni, X. Morkoc, H. Son, K. -A. TI Current versus voltage characteristics of GaN/AlGaN/GaN double heterostructures with varying AlGaN thickness and composition under hydrostatic pressure SO JOURNAL OF APPLIED PHYSICS LA English DT Article ID 2-DIMENSIONAL ELECTRON GASES; PIEZOELECTRIC POLARIZATION; UNIAXIAL-STRESS; CONDUCTIVITY; GAN AB We have studied current versus voltage characteristics of n-GaN/u-AlGaN/n-GaN double heterostructure devices under hydrostatic pressure up to 500 MPa. Devices were grown on c-plane sapphire substrates by organometallic vapor phase epitaxy using epitaxial layer overgrowth. The effect of AlGaN layer thickness and composition on the pressure sensitivity was investigated. For a fixed applied bias, we found that the current decreases approximately linearly in magnitude with increasing hydrostatic pressure over the range of voltages and pressures applied. The decrease in current magnitude can be attributed to piezoelectric effects and is consistent with model calculations. The polarization charge densities at the GaN/AlGaN interfaces change with hydrostatic pressure, which in turn modifies the internal potential barrier. Changes in the AlGaN layer thickness and composition also modify the interfacial polarization, with thicker AlGaN layers and higher AlN content increasing the effect of pressure on the observed current versus voltage characteristics. The strain gauge factors obtained for these devices range from similar to 200 to 800. (c) 2008 American Institute of Physics. C1 [Steinke, I. P.; Ruden, P. P.] Univ Minnesota, Dept Elect & Comp Engn, Minneapolis, MN 55455 USA. [Ni, X.; Morkoc, H.] Virginia Commonwealth Univ, Dept Elect Engn, Richmond, VA 23284 USA. [Son, K. -A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Steinke, IP (reprint author), Univ Minnesota, Dept Elect & Comp Engn, Minneapolis, MN 55455 USA. EM stei0194@umn.edu RI Ni, Xianfeng/A-1635-2011 NR 17 TC 3 Z9 3 U1 0 U2 14 PU AMER INST PHYSICS PI MELVILLE PA CIRCULATION & FULFILLMENT DIV, 2 HUNTINGTON QUADRANGLE, STE 1 N O 1, MELVILLE, NY 11747-4501 USA SN 0021-8979 J9 J APPL PHYS JI J. Appl. Phys. PD MAR 15 PY 2008 VL 103 IS 6 AR 064502 DI 10.1063/1.2844484 PG 6 WC Physics, Applied SC Physics GA 281ZH UT WOS:000254536900118 ER PT J AU Wu, LG Wang, B AF Wu, Liguang Wang, Bin TI What has changed the proportion of intense hurricanes in the last 30 years? SO JOURNAL OF CLIMATE LA English DT Article ID VERTICAL WIND SHEAR; TROPICAL CYCLONES; ATLANTIC; INCREASE; CLIMATE; MODEL AB The recently reported increase in the proportion of intense hurricanes is considerably larger than those projected by the maximum potential intensity (MPI) theory and the results of numerical simulation. To reconcile this discrepancy, the authors examined the best-track datasets for the North Atlantic (NA), western North Pacific (WNP), and eastern North Pacific (ENP) basins. It was found that the changes in the tropical cyclone formation locations and prevailing tracks may have contributed to the changes in the proportion of the intense hurricanes over the past 30 yr. The authors suggest that the changes in the formation locations and prevailing tracks have a profound impact on the basinwide tropical cyclone intensity. Thus, how the atmospheric circulation in the tropical cyclone basins responds to the global warming may be a critical factor in understanding the impacts of global warming on tropical cyclone intensity. C1 [Wu, Liguang] NASA, Goddard Space Flight Ctr, Atmospheres Lab, Greenbelt, MD 20071 USA. [Wu, Liguang] Univ Maryland, Goddard Earth & Technol Ctr, Baltimore, MD 21201 USA. [Wang, Bin] Univ Hawaii Manoa, Dept Meteorol, Honolulu, HI 96822 USA. [Wang, Bin] Univ Hawaii Manoa, IPRC, Honolulu, HI 96822 USA. [Wang, Bin] Ocean Univ China, Coll Phys & Environm Oceanog, Qingdao 266003, Peoples R China. RP Wu, LG (reprint author), NASA, Goddard Space Flight Ctr, Atmospheres Lab, Code 613-1, Greenbelt, MD 20071 USA. EM liguang@agnes.gsfc.nasa.gov NR 25 TC 27 Z9 31 U1 0 U2 6 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 0894-8755 EI 1520-0442 J9 J CLIMATE JI J. Clim. PD MAR 15 PY 2008 VL 21 IS 6 BP 1432 EP 1439 DI 10.1175/2007JCLI1715.1 PG 8 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 280IY UT WOS:000254421100017 ER PT J AU Erickson, DJ Mills, RT Gregg, J Blasing, TJ Hoffman, FM Andres, RJ Devries, M Zhu, Z Kawa, SR AF Erickson, D. J., III Mills, R. T. Gregg, J. Blasing, T. J. Hoffman, F. M. Andres, R. J. Devries, M. Zhu, Z. Kawa, S. R. TI An estimate of monthly global emissions of anthropogenic CO(2): Impact on the seasonal cycle of atmospheric CO(2) SO JOURNAL OF GEOPHYSICAL RESEARCH-BIOGEOSCIENCES LA English DT Article ID CARBON-DIOXIDE EMISSIONS; TRANSPORT; LAND AB Monthly estimates of the global emissions of anthropogenic CO(2) are presented. Approximating the seasonal CO(2) emission cycle using a 2-harmonic Fourier series with coefficients as a function of latitude, the annual fluxes are decomposed into monthly flux estimates based on data for the United States and applied globally. These monthly anthropogenic CO(2) flux estimates are then used to model atmospheric CO(2) concentrations using meteorological fields from the NASA GEOS-4 data assimilation system. We find that the use of monthly resolved fluxes makes a significant difference in the seasonal cycle of atmospheric CO(2) in and near those regions where anthropogenic CO(2) is released to the atmosphere. Local variations of 2-6 ppmv CO(2) in the seasonal cycle amplitude are simulated; larger variations would be expected if smaller source-receptor distances could be more precisely specified using a more refined spatial resolution. We also find that in the midlatitudes near the sources, synoptic scale atmospheric circulations are important in the winter and that boundary layer venting and diurnal rectifier effects are more important in the summer. These findings have implications for inverse-modeling efforts that attempt to estimate surface source/sink regions especially when the surface sinks are colocated with regions of strong anthropogenic CO(2) emissions. C1 [Erickson, D. J., III; Mills, R. T.; Hoffman, F. M.; Devries, M.] Oak Ridge Natl Lab, Div Math & Comp Sci, Computat Earth Sci Grp, Oak Ridge, TN 37831 USA. [Erickson, D. J., III] Duke Univ, Nicholas Sch Environm & Earth Sci, Durham, NC USA. [Gregg, J.] Univ Maryland, Dept Geog, College Pk, MD 20742 USA. [Blasing, T. J.; Andres, R. J.] Oak Ridge Natl Lab, Div Environm Sci, Oak Ridge, TN 37831 USA. [Devries, M.] Vanderbilt Univ, Sch Engn, Nashville, TN USA. [Zhu, Z.; Kawa, S. R.] NASA, Goddard Space Flight Ctr, Atmospheres Lab, Greenbelt, MD 20771 USA. RP Erickson, DJ (reprint author), Oak Ridge Natl Lab, Div Math & Comp Sci, Computat Earth Sci Grp, Oak Ridge, TN 37831 USA. RI Gregg, Jay/C-6732-2011; Blasing, T/B-9498-2012; ANDRES, ROBERT/B-9786-2012; Kawa, Stephan/E-9040-2012; Hoffman, Forrest/B-8667-2012; OI Gregg, Jay/0000-0003-3946-3099; Hoffman, Forrest/0000-0001-5802-4134; ANDRES, ROBERT/0000-0001-8781-4979 NR 23 TC 15 Z9 15 U1 0 U2 6 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 MAR 15 PY 2008 VL 113 IS G1 AR G01023 DI 10.1029/2007JG000435 PG 10 WC Environmental Sciences; Geosciences, Multidisciplinary SC Environmental Sciences & Ecology; Geology GA 276TQ UT WOS:000254166400002 ER PT J AU Jolliff, JK Kindle, JC Penta, B Helber, R Lee, ZP Shulman, I Arnone, R Rowley, CD AF Jolliff, Jason K. Kindle, John C. Penta, Bradley Helber, Robert Lee, Zhongping Shulman, Igor Arnone, Robert Rowley, Clark D. TI On the relationship between satellite-estimated bio-optical and thermal properties in the Gulf of Mexico SO JOURNAL OF GEOPHYSICAL RESEARCH-BIOGEOSCIENCES LA English DT Review ID DISSOLVED ORGANIC-MATTER; WEST FLORIDA SHELF; SEA-SURFACE TEMPERATURE; NITRATE-DEPLETION TEMPERATURES; MISSISSIPPI RIVER PLUME; OCEAN-COLOR DATA; CHLOROPHYLL-A; PHYTOPLANKTON BIOMASS; CONTINENTAL-MARGIN; LIGHT-ABSORPTION AB Three years of Sea-viewing Wide Field-of-view Sensor (SeaWiFS) ocean color data were combined with three-dimensional thermal fields generated by the U. S. Navy's Modular Ocean Data Assimilation System (MODAS) in order to examine the interdependencies between bio-optical fields and their relationship to seasonal and mesoscale changes in upper ocean thermal structure. The combined data set suggests that the oceanic boundary layer within the Gulf of Mexico may be broadly defined by two seasonally occurring bio-thermal periods. A winter mixing period, characterized by net heat losses to the atmosphere, deepening of the isothermal layer depth, and annual maxima of satellite-estimated colored detrital matter (CDM) absorption coefficients and surface pigment concentration, was followed by a thermally stratified period characterized by net surface ocean heating, reduced isothermal layer depths, and annual minima in surface bio-optical fields. Variability in the interdependencies of ocean color products was used to diagnose an attendant shift in the size-structure of surface phytoplankton communities as well as identify CDM as the constituent responsible for the majority of blue-light absorption in Gulf of Mexico surface waters. The mesoscale circulation, as resolved by MODAS thermal fields into cold and warm-core eddies, appears to significantly modulate the seasonal bio-optical cycle of CDM absorption and surface pigment concentration. An empirical model was developed to describe CDM absorption as a function of upper ocean thermal energy. The model accounted for nearly half the variance in the satellite-estimate of this bio-optical variable. Large mismatches between the model and satellite data implied episodes of shelf water export to the deep Gulf of Mexico. C1 [Jolliff, Jason K.; Kindle, John C.; Penta, Bradley; Helber, Robert; Lee, Zhongping; Shulman, Igor; Arnone, Robert; Rowley, Clark D.] USN, Res Lab, Stennis Space Ctr, Stennis Space Ctr, MS 39529 USA. RP Jolliff, JK (reprint author), USN, Res Lab, Stennis Space Ctr, Stennis Space Ctr, MS 39529 USA. EM jason.jolliff@nrlssc.navy.mil OI Rowley, Clark/0000-0003-3496-6404 NR 136 TC 11 Z9 11 U1 1 U2 7 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-8953 EI 2169-8961 J9 J GEOPHYS RES-BIOGEO JI J. Geophys. Res.-Biogeosci. PD MAR 15 PY 2008 VL 113 IS G1 AR G01024 DI 10.1029/2006JG000373 PG 27 WC Environmental Sciences; Geosciences, Multidisciplinary SC Environmental Sciences & Ecology; Geology GA 276TQ UT WOS:000254166400001 ER PT J AU Bhatt, RT Choi, SR Cosgriff, LM Fox, DS Lee, KN AF Bhatt, Ramakrishna T. Choi, Sung R. Cosgriff, Laura M. Fox, Dennis-S. Lee, Kang N. TI Impact resistance of environmental barrier coated SiC/SiC composites SO MATERIALS SCIENCE AND ENGINEERING A-STRUCTURAL MATERIALS PROPERTIES MICROSTRUCTURE AND PROCESSING LA English DT Article DE impact; EBC coatings; SiC/SiC composites; mechanical properties; NDE ID SIO2 SCALE VOLATILITY; SILICON-CARBIDE; COMBUSTION CONDITIONS; COATINGS; DAMAGE; OXIDATION; MULLITE; MODEL AB Impact performance of 2D woven SiC/SiC composites coated with 225 and 525 mu m thick environmental barrier coating (EBC) was investigated. The composites were fabricated by melt infiltration and the EBC was deposited by plasma spray. Impact tests were conducted at room temperature and at 1316 degrees C in air using 1.59 mm diameter steel-balls at projectile velocities ranging from 110 to 375 m/s. Both microscopy and non-destructive evaluation (NDE) methods were used to determine the extent of damage in the substrate and coating with increasing projectile velocity. The impacted specimens were tensile tested at room temperature to determine their residual mechanical properties. At projectile velocities less than 125 m/s, no detectable internal damage was noticed in the MI SiC/SiC composites coated with 525 mu m EBC. With increase in projectile velocity beyond this value. spallation of EBC layers, delamination of fiber plies, and fiber fracture were detected. At a fixed projectile velocity, the composites coated with 525 mu m EBC showed less damage than those coated with 225 mu m EBC. Both types of coated composites retained a large fraction of the baseline proper-ties of the as-fabricated composites and exhibited non-brittle failure after impact testing. Furnace exposure of impacted specimens in a moisture environment at 1316 degrees C for 500 h indicated that the through-the-thickness cracks in the coating and delamination cracks in the substrate generated after impact testing acted as conduits for internal oxidation. (C) 2007 Elsevier B.V. All rights reserved. C1 [Bhatt, Ramakrishna T.; Fox, Dennis-S.] NASA Glenn Res Ctr, USA Vehicle Technol Directorate, Cleveland, OH 44135 USA. [Choi, Sung R.] Naval Air Syst Command, Patuxent River, MD 20670 USA. [Cosgriff, Laura M.] Cleveland State Univ, Cleveland, OH 44115 USA. [Lee, Kang N.] Rolls Royce Corp, Indianapolis, IN 46206 USA. RP Bhatt, RT (reprint author), NASA Glenn Res Ctr, USA Vehicle Technol Directorate, Cleveland, OH 44135 USA. EM Ramakrishna.T.Bhatt@nasa.gov NR 20 TC 24 Z9 27 U1 4 U2 37 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 MAR 15 PY 2008 VL 476 IS 1-2 BP 8 EP 19 DI 10.1016/j.msea.2007.04.067 PG 12 WC Nanoscience & Nanotechnology; Materials Science, Multidisciplinary; Metallurgy & Metallurgical Engineering SC Science & Technology - Other Topics; Materials Science; Metallurgy & Metallurgical Engineering GA 270AX UT WOS:000253693200002 ER PT J AU Bhatt, RT Choi, SR Cosgriff, LM Fox, DS Lee, KN AF Bhatt, Ramakrishna T. Choi, Sung R. Cosgriff, Laura M. Fox, Dennis S. Lee, Kang N. TI Impact resistance of uncoated SiC/SiC composites SO MATERIALS SCIENCE AND ENGINEERING A-STRUCTURAL MATERIALS PROPERTIES MICROSTRUCTURE AND PROCESSING LA English DT Article DE impact; SiC/SiC composite; NDE; mechanical properties ID ENVIRONMENTAL BARRIER COATINGS; SIO2 SCALE VOLATILITY; COMBUSTION CONDITIONS; SILICON-NITRIDE; DAMAGE BEHAVIOR; MODEL AB Two-dimensional woven SiC/SiC composites fabricated by melt infiltration method were impact tested at room temperature and at 1316 degrees C in air using 1.59-mm diameter steel-ball projectiles at velocities ranging from 115 to 400 m/s. The extent of substrate damage with increasing projectile velocity was imaged and analyzed using optical and scanning electron microscopy, and non-destructive evaluation (NDE) methods such as pulsed thermography, and computed tomography. The impacted specimens were tensile tested at room temperature to determine their residual mechanical properties. Results indicate that at 115 m/s projectile velocity, the composite showed no noticeable surface or internal damage and retained its as-fabricated mechanical properties. As the projectile velocity increased above this value, the internal damage increased and mechanical properties degraded. At velocities >300 m/s, the projectile penetrated through the composite, but the composite retained similar to 50% of the ultimate tensile strength of the as-fabricated composite and exhibited non-brittle failure. Predominant internal damages are delamination of fiber plies, fiber fracture and matrix shearing, (C) 2007 Elsevier B.V. All rights reserved. C1 [Bhatt, Ramakrishna T.; Fox, Dennis S.] NASA Glenn Res Ctr, USA Vehicle Technol Directorate, Cleveland, OH 44135 USA. [Choi, Sung R.] Naval Air Syst Command, Patuxent River, MD 20670 USA. [Cosgriff, Laura M.] Cleveland State Univ, Cleveland, OH 44115 USA. [Lee, Kang N.] Rolls Royce Corp, Indianapolis, IN 46206 USA. RP Bhatt, RT (reprint author), NASA Glenn Res Ctr, USA Vehicle Technol Directorate, Cleveland, OH 44135 USA. EM Ramakrishna.T.Bhatt@nasa.gov NR 20 TC 20 Z9 22 U1 1 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 MAR 15 PY 2008 VL 476 IS 1-2 BP 20 EP 28 DI 10.1016/j.msea.2007.04.066 PG 9 WC Nanoscience & Nanotechnology; Materials Science, Multidisciplinary; Metallurgy & Metallurgical Engineering SC Science & Technology - Other Topics; Materials Science; Metallurgy & Metallurgical Engineering GA 270AX UT WOS:000253693200003 ER PT J AU Bansal, NP Zhu, DM AF Bansal, Narottam P. Zhu, Dongming TI Thermal properties of oxides with magnetoplumbite structure for advanced thermal barrier coatings SO SURFACE & COATINGS TECHNOLOGY LA English DT Article DE magnetoplumbite oxides; thermal conductivity; thermal expansion; thermal barrier coatings; doping ID LANTHANUM HEXAALUMINATE; CONDUCTIVITY AB Oxides having magnetoplumbite structure are promising candidate materials for applications as high temperature thermal barrier coatings because of their high thermal stability, high thermal expansion, and low thermal conductivity. In this study, powders of LaMgAl11O19, GdMgAl11O19, SmMgAl11O19, and Gd0.7Yb0.3MgAl11O19 magnetoplumbite oxides were synthesized by citric acid sol-gel method and hot-pressed into disk specimens. The thermal expansion coefficients (CTE) of these oxide materials were measured from room temperature to 1500 degrees C. The average CTE value was found to be similar to 9.6 x 10(-6)/C. Thermal conductivity of these magnetoplumbite-based oxide materials was also evaluated using steady-state laser heat flux test method. The effects of doping on thermal properties were also examined. Thermal conductivity of the doped Gd0.7Yb0.3MgAl11O19 composition was found to be lower than that of the undoped GdMgAl11O19. In contrast, thermal expansion coefficient was found to be independent of the oxide composition and appears to be controlled by the magnetoplumbite crystal structure. Preliminary results of thermal conductivity testing at 1600 degrees C for LaMgAl11O19 and LaMnAl11O19 magnetoplumbite oxide coatings plasma-sprayed on NiCrAlY/Rene N5 superalloy substrates are also presented. The plasma-sprayed coatings did not sinter even. at temperatures as high as 1600 degrees C. Published by Elsevier B.V. C1 NASA, Glenn Res Ctr, Struct & Mat Div, Cleveland, OH 44135 USA. [Zhu, Dongming] Glenn Res Ctr, US Army Lab, Vehicle Technol Directorate, Cleveland, OH 44135 USA. RP Bansal, NP (reprint author), NASA, Glenn Res Ctr, Struct & Mat Div, Cleveland, OH 44135 USA. EM Narottam.P.Bansal@nasa.gov NR 15 TC 56 Z9 64 U1 2 U2 40 PU ELSEVIER SCIENCE SA PI LAUSANNE PA PO BOX 564, 1001 LAUSANNE, SWITZERLAND SN 0257-8972 J9 SURF COAT TECH JI Surf. Coat. Technol. PD MAR 15 PY 2008 VL 202 IS 12 BP 2698 EP 2703 DI 10.1016/j.surfcoat.2007.09.048 PG 6 WC Materials Science, Coatings & Films; Physics, Applied SC Materials Science; Physics GA 279PT UT WOS:000254367800025 ER PT J AU Garcia, M Peters-Lidard, CD Goodrich, DC AF Garcia, Matthew Peters-Lidard, Christa D. Goodrich, David C. TI Spatial interpolation of precipitation in a dense gauge network for monsoon storm events in the southwestern United States SO WATER RESOURCES RESEARCH LA English DT Article ID MESOSCALE CONVECTIVE SYSTEMS; NORTH-AMERICAN MONSOON; MULTIQUADRIC INTERPOLATION; ALPINE PRECIPITATION; RAINFALL VARIABILITY; HIGH-RESOLUTION; POINT RAINFALL; UNCERTAINTY; MODEL; SCALE AB Inaccuracy in spatially distributed precipitation fields can contribute significantly to the uncertainty of hydrological states and fluxes estimated from land surface models. This paper examines the results of selected interpolation methods for both convective and mixed/stratiform events that occurred during the North American monsoon season over a dense gauge network at the U. S. Department of Agriculture Agricultural Research Service Walnut Gulch Experimental Watershed in the southwestern United States. The spatial coefficient of variation for the precipitation field is employed as an indicator of event morphology, and a gauge clustering factor CF is formulated as a new, scale-independent measure of network organization. We consider that CF < 0 ( a more distributed gauge network) will produce interpolation errors by reduced resolution of the precipitation field and that CF > 0 ( clustering in the gauge network) will produce errors because of reduced areal representation of the precipitation field. Spatial interpolation is performed using both inverse-distance-weighted (IDW) and multiquadric-biharmonic (MQB) methods. We employ ensembles of randomly selected network subsets for the statistical evaluation of interpolation errors in comparison with the observed precipitation. The magnitude of interpolation errors and differences in accuracy between interpolation methods depend on both the density and the geometrical organization of the gauge network. Generally, MQB methods outperform IDW methods in terms of interpolation accuracy under all conditions, but it is found that the order of the IDW method is important to the results and may, under some conditions, be just as accurate as the MQB method. In almost all results it is demonstrated that the inverse-distance-squared method for spatial interpolation, commonly employed in operational analyses and for engineering assessments, is inferior to the ID- cubed method, which is also more computationally efficient than the MQB method in studies of large networks. C1 [Garcia, Matthew] Univ Maryland Baltimore Cty, Good Earth Sci & Technol Ctr, Baltimore, MD 21228 USA. [Garcia, Matthew; Peters-Lidard, Christa D.] NASA, Goddard Space Flight Ctr, Hydrol Sci Branch, Greenbelt, MD 20771 USA. [Goodrich, David C.] ARS, SW Watershed Res Ctr, USDA, Tucson, AZ 85719 USA. RP Garcia, M (reprint author), Univ Maryland Baltimore Cty, Good Earth Sci & Technol Ctr, Baltimore, MD 21228 USA. EM matthew.garcia@nasa.gov RI Goodrich, David/B-1763-2009; Garcia, Matthew/K-9286-2013; Peters-Lidard, Christa/E-1429-2012 OI Goodrich, David/0000-0001-7735-1448; Garcia, Matthew/0000-0002-9637-4204; Peters-Lidard, Christa/0000-0003-1255-2876 NR 63 TC 33 Z9 34 U1 1 U2 12 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 MAR 15 PY 2008 VL 44 IS 5 AR W05S13 DI 10.1029/2006WR005788 PG 14 WC Environmental Sciences; Limnology; Water Resources SC Environmental Sciences & Ecology; Marine & Freshwater Biology; Water Resources GA 276UZ UT WOS:000254170300001 ER PT J AU Korotova, GI Sibeck, DG Rosenberg, T AF Korotova, G. I. Sibeck, D. G. Rosenberg, T. TI Seasonal dependence of Interball flux transfer events SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID INTERPLANETARY MAGNETIC-FIELD; MAGNETOPAUSE; RECONNECTION AB J. Raeder ( 2006) presented the results of a global magnetohydrodynamic simulation indicating that flux transfer events ( FTEs) form solely in the winter hemisphere and move poleward in the direction of the background magnetosheath flow during periods of strongly southward interplanetary magnetic field ( IMF) orientation. This paper presents results from a statistical survey of flux transfer FTEs observed on the mid-latitude northern and southern magnetopause by the magnetometer on the Interball-1 spacecraft over the course of its five-year mission from 1995 to 1999. Interball-1 observations confirm that FTEs exhibit a strong tendency to occur in the winter hemisphere. C1 [Rosenberg, T.] Univ Maryland, IPST, College Pk, MD 20742 USA. [Sibeck, D. G.] NASA GSFC, Greenbelt, MD 20723 USA. [Korotova, G. I.] IZMIRAN, Troitsk 142190, Russia. RP Korotova, GI (reprint author), Univ Maryland, IPST, College Pk, MD 20742 USA. EM korotova@excite.com RI Sibeck, David/D-4424-2012 NR 19 TC 6 Z9 6 U1 0 U2 0 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD MAR 14 PY 2008 VL 35 IS 5 AR L05106 DI 10.1029/2008GL033254 PG 4 WC Geosciences, Multidisciplinary SC Geology GA 276TG UT WOS:000254165400007 ER PT J AU Mackenzie, RA Iess, L Tortora, P Rappaport, NJ AF Mackenzie, R. A. Iess, L. Tortora, P. Rappaport, N. J. TI A non-hydrostatic Rhea SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article AB Radiometric data obtained during Cassini's close flyby of Rhea, on 26 November 2005, has been subject to several published analyses aiming to determine the satellite's mass and quadrupole gravity moments. Combining aspects of two of these analyses we present our best, unbiased estimates of the gravity field parameters and point out how the constraint of hydrostatic equilibrium adopted by previous analysts affects the results. We present solutions based on a broad range of geophysical assumptions, such as the presence of degree 3 and 4 gravity field constrained at different levels. The result is a balanced approach which describes our current knowledge of Rhea's gravity field. In the case of a gravity field limited to second degree harmonics the most reliable estimates are GM = 153.9398 +/- 0.0008 km(3) s(-2), 10(6) J(2) = 931.0 +/- 12.0, 10(6) C(22) = 237.2 +/- 4.5, and 10(6) S(22) = 3.8 +/- 3.8. C1 [Iess, L.] Univ Roma La Sapienza, Dipartimento Ingn Aerosp & Astronaut, I-00185 Rome, Italy. [Tortora, P.] Univ Bologna, Fac Ingn 2, DIEM, I-47100 Forli, Italy. [Mackenzie, R. A.; Rappaport, N. J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Mackenzie, RA (reprint author), European Space Technol Ctr, Robert Bosch Str 5, D-64293 Darmstadt, Germany. EM ruaraidh.mackenzie@esa.int RI IESS, Luciano/F-4902-2011; Tortora, Paolo/J-6191-2012 OI IESS, Luciano/0000-0002-6230-5825; Tortora, Paolo/0000-0001-9259-7673 NR 5 TC 12 Z9 12 U1 0 U2 1 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD MAR 14 PY 2008 VL 35 IS 5 AR L05204 DI 10.1029/2007GL032898 PG 5 WC Geosciences, Multidisciplinary SC Geology GA 276TG UT WOS:000254165400005 ER PT J AU Stammerjohn, SE Martinson, DG Smith, RC Yuan, X Rind, D AF Stammerjohn, S. E. Martinson, D. G. Smith, R. C. Yuan, X. Rind, D. TI Trends in Antarctic annual sea ice retreat and advance and their relation to El Nino-Southern Oscillation and Southern Annular Mode variability SO JOURNAL OF GEOPHYSICAL RESEARCH-OCEANS LA English DT Article ID HEMISPHERE CLIMATE-CHANGE; ATMOSPHERIC CIRCULATION; PENINSULA REGION; BELLINGSHAUSEN SEAS; SPATIAL PATTERNS; OCEAN CLIMATE; ENSO; TEMPERATURE; PRECIPITATION; IMPACT AB Previous studies have shown strong contrasting trends in annual sea ice duration and in monthly sea ice concentration in two regions of the Southern Ocean: decreases in the western Antarctic Peninsula/southern Bellingshausen Sea ( wAP/sBS) region and increases in the western Ross Sea ( wRS) region. To better understand the evolution of these regional sea ice trends, we utilize the full temporal ( quasi-daily) resolution of satellite-derived sea ice data to track spatially the annual ice edge advance and retreat from 1979 to 2004. These newly analyzed data reveal that sea ice is retreating 31 +/- 10 days earlier and advancing 54 +/- 9 days later in the wAP/sBS region ( i.e., total change over 1979 - 2004), whereas in the wRS region, sea ice is retreating 29 +/- 6 days later and advancing 31 +/- 6 days earlier. Changes in the wAP/sBS and wRS regions, particularly as observed during sea ice advance, occurred in association with decadal changes in the mean state of the Southern Annular Mode ( SAM; negative in the 1980s and positive in the 1990s) and the high-latitude response to El Nino - Southern Oscillation ( ENSO). In general, the high-latitude ice-atmosphere response to ENSO was strongest when - SAM was coincident with El Nino and when +SAM was coincident with La Nina, particularly in the wAP/sBS region. In total, there were 7 of 11 -SAMs between 1980 and 1990 and the 7 of 10 +SAMs between 1991 and 2000 that were associated with consistent decadal sea ice changes in the wAP/sBS and wRS regions, respectively. Elsewhere, ENSO/SAM-related sea ice changes were not as consistent over time ( e. g., western Weddell, Amundsen, and eastern Ross Sea region), or variability in general was high ( e. g., central/ eastern Weddell and along East Antarctica). C1 [Stammerjohn, S. E.; Martinson, D. G.; Yuan, X.] Columbia Univ, Lamont Doherty Earth Observ, Palisades, NY 10964 USA. [Stammerjohn, S. E.; Martinson, D. G.] Columbia Univ, Dept Earth & Environm Sci, New York, NY USA. [Smith, R. C.] Univ Calif Santa Barbara, Inst Computat Earth Syst Sci, Santa Barbara, CA 93106 USA. [Smith, R. C.] Univ Calif Santa Barbara, Dept Geog, Santa Barbara, CA 93106 USA. [Rind, D.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA. RP Stammerjohn, SE (reprint author), Columbia Univ, Lamont Doherty Earth Observ, Palisades, NY 10964 USA. EM sstammerjohn@giss.nasa.gov OI STAMMERJOHN, SHARON/0000-0002-1697-8244 NR 84 TC 261 Z9 268 U1 3 U2 84 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 MAR 14 PY 2008 VL 113 IS C3 AR C03S90 DI 10.1029/2007JC004269 PG 20 WC Oceanography SC Oceanography GA 276UB UT WOS:000254167600003 ER PT J AU Bonifacie, M Jendrzejewski, N Agrinier, P Humler, E Coleman, M Javoy, M AF Bonifacie, M. Jendrzejewski, N. Agrinier, P. Humler, E. Coleman, M. Javoy, M. TI The chlorine isotope composition of Earth's mantle SO SCIENCE LA English DT Article ID SEA-FLOOR SERPENTINITES; MIDOCEAN RIDGE BASALTS; OCEANIC-CRUST; BENEATH; BEHAVIOR; FLUIDS; FRACTIONATION; ASSIMILATION; EVAPORITES; ATLANTIC AB Chlorine stable isotope compositions ( delta Cl-37) of 22 mid- ocean ridge basalts ( MORBs) correlate with Cl content. The high-delta Cl-37, Cl- rich basalts are highly contaminated by Cl- rich materials ( seawater, brines, or altered rocks). The low-delta(37) Cl, Cl- poor basalts approach the composition of uncontaminated, mantle- derived magmas. Thus, most or all oceanic lavas are contaminated to some extent during their emplacement. MORB- source mantle has delta(37) Cl <= -1.6 per mil (%), which is significantly lower than that of surface reservoirs (similar to 0 parts per thousand not equal). This isotopic difference between the surface and deep Earth results from net Cl isotopic fractionation ( associated with removal of Cl from the mantle and its return by subduction over Earth history) and/ or the addition ( to external reservoirs) of a late volatile supply that is Cl-37- enriched. C1 [Bonifacie, M.; Jendrzejewski, N.; Agrinier, P.; Humler, E.; Javoy, M.] Inst Phys Globe, CNRS INSU, UMR 7154, F-75251 Paris 05, France. [Bonifacie, M.; Jendrzejewski, N.; Agrinier, P.; Javoy, M.] UPD, CNRS INSU, UMR 7154, F-75251 Paris, France. [Bonifacie, M.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. [Humler, E.] Univ Nantes, Lab Planetol & Geodynam, CNRS, UMR 6112, F-44322 Nantes 3, France. [Coleman, M.] Univ Reading, Sch Human & Environm Sci, Reading RG6 6AB, Berks, England. [Coleman, M.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Bonifacie, M (reprint author), Inst Phys Globe, CNRS INSU, UMR 7154, 4 Pl Jussieu, F-75251 Paris 05, France. EM bonifaci@gps.caltech.edu RI Bonifacie, Magali/A-5656-2011; Coleman, Max/A-1303-2007 OI Coleman, Max/0000-0002-5514-1826 NR 26 TC 50 Z9 50 U1 2 U2 37 PU AMER ASSOC ADVANCEMENT SCIENCE PI WASHINGTON PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 USA SN 0036-8075 J9 SCIENCE JI Science PD MAR 14 PY 2008 VL 319 IS 5869 BP 1518 EP 1520 DI 10.1126/science.1150988 PG 3 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 273PI UT WOS:000253943800036 PM 18339936 ER PT J AU Farrell, WM Stubbs, TJ Halekas, JS Delory, GT Collier, MR Vondrak, RR Lin, RP AF Farrell, W. M. Stubbs, T. J. Halekas, J. S. Delory, G. T. Collier, M. R. Vondrak, R. R. Lin, R. P. TI Loss of solar wind plasma neutrality and affect on surface potentials near the lunar terminator and shadowed polar regions SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID IN-CELL SIMULATIONS; WAKE; EXPANSION; VACUUM AB As the solar wind is absorbed on the lunar dayside, a clear and obvious plasma void is created in the anti-solar direction that extends many lunar radii behind the Moon. Plasma adjacent to this void will expand into the depleted region and this process is modeled here using a particle-in-cell code. It is found that thermal electrons will diffuse into the void ahead of the ions, creating a break in plasma quasi-neutrality. In essence, immediately trailing behind the lunar terminator/ polar regions, there is a magnetic-field aligned E-field peaking near 400 mV/ m associated with a standing double-layer, this layer consisting of fast thermal electrons ( electron cloud) moving into the central void ahead of an ion-enhanced layer. We demonstrate that the surface locations that are incident with the electron cloud ( just nightside of the terminator) will develop enhanced negative surface potentials due to the dominance of electron currents. Such regions of large negative potentials near the lunar poles are of interest, especially given NASA's recent announcement of a lunar outpost at the south polar Aitken Basin. C1 [Farrell, W. M.; Stubbs, T. J.; Collier, M. R.; Vondrak, R. R.] NASA, Goddard Space Flight Ctr, Solar Syst Explorat Div, Greenbelt, MD 20771 USA. [Halekas, J. S.; Delory, G. T.; Lin, R. P.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Stubbs, T. J.] Univ Maryland, Goddard Earth Sci & Technol Ctr, Baltimore, MD 21201 USA. RP Farrell, WM (reprint author), NASA, Goddard Space Flight Ctr, Solar Syst Explorat Div, Code 661, Greenbelt, MD 20771 USA. EM william.farrell@gsfc.nasa.gov RI Collier, Michael/I-4864-2013; Stubbs, Timothy/I-5139-2013; Farrell, William/I-4865-2013; OI Collier, Michael/0000-0001-9658-6605; Stubbs, Timothy/0000-0002-5524-645X; Halekas, Jasper/0000-0001-5258-6128 NR 14 TC 20 Z9 20 U1 0 U2 1 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD MAR 13 PY 2008 VL 35 IS 5 AR L05105 DI 10.1029/2007GL032653 PG 5 WC Geosciences, Multidisciplinary SC Geology GA 276TF UT WOS:000254165200002 ER PT J AU Yan, XH Jo, YH Jiang, L Wan, ZW Liu, WT Li, Y Zhan, JM Du, T AF Yan, Xiao-Hai Jo, Young-Heon Jiang, Lide Wan, Zhenwen Liu, W. Timothy Li, Yan Zhan, Jiemin Du, Tao TI Impact of the Three Gorges Dam water storage on the Yangtze River outflow into the East China Sea SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article AB The role of the Three Gorges Dam Water Storage ( TGDWS) in changing salinity in the East China Sea ( ECS) near the Yangtze River Estuary ( YRE) was investigated using a multi-sensor remote sensing technique, namely the salt steric height anomaly, calculated from Sea Surface Height Anomaly ( SSHA) and Sea Surface Temperature ( SST) data. The patterns of the salt steric height anomaly near the YRE agreed well with the in situ Sea Surface Salinity ( SSS) measurements. In order to examine the changes in stability in the mixed layer near the YRE due to TGDWS, the time series of the steric height anomaly ratio ( R(s)') between heat and salt at three locations were estimated. The R(s)' was strongly associated with a coastal upwelling in the ECS, because the reduced freshwater outflow gives rise to changes of both mixed layer depth and surface current patterns off the YRE. C1 [Yan, Xiao-Hai; Jo, Young-Heon; Jiang, Lide; Du, Tao] Univ Delaware, Grad Coll Marine & Earth Studies, Ctr Remote Sensing, Newark, DE 19716 USA. [Yan, Xiao-Hai; Wan, Zhenwen; Li, Yan] Xiamen Univ, State Key Lab Marine Environm Sci, Xiamen 361005, Peoples R China. [Liu, W. Timothy] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Zhan, Jiemin] Zhongshan Univ, Dept Appl Mech & Engn, Guangzhou 510275, Peoples R China. RP Yan, XH (reprint author), Univ Delaware, Grad Coll Marine & Earth Studies, Ctr Remote Sensing, Newark, DE 19716 USA. EM xiaohai@udel.edu RI Li, Y/G-3453-2010; Jiang, Lide/G-2041-2010 OI Jiang, Lide/0000-0002-9883-4411 NR 13 TC 11 Z9 11 U1 3 U2 26 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD MAR 13 PY 2008 VL 35 IS 5 AR L05610 DI 10.1029/2007GL032908 PG 5 WC Geosciences, Multidisciplinary SC Geology GA 276TF UT WOS:000254165200004 ER PT J AU O'Neill, NT Eck, TF Reid, JS Smirnov, A Pancrati, O AF O'Neill, N. T. Eck, T. F. Reid, J. S. Smirnov, A. Pancrati, O. TI Coarse mode optical information retrievable using ultraviolet to short-wave infrared sun photometry: Application to United Arab Emirates unified aerosol experiment data SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID DEPTH; SPHEROIDS AB The United Arab Emirates Unified Aerosol experiment provided a unique opportunity for testing aerosol retrieval algorithms in conditions where the optical influence of coarse mode particles was significant. Comparisons between Aerosol Robotic Network (AERONET) Sun photometry retrievals of a previously reported spectral deconvolution algorithm (SDA) and surface-based microphysical and optical measurements showed levels of correlation suggestive of moderate vertical homogeneity for (extensive) measures of fine and coarse mode aerosol particles and stronger vertical homogeneity for indicators of (intensive) aerosol type. An extension of the SDA into the short-wave infrared (SDA+) was developed in order to exploit the enhanced coarse mode information available in new AERONET instruments which include a 1.64 mu m channel. Comparisons between values of coarse mode Angstrom exponent alpha(c) (1.64 mu m)) retrieved from SDA+ and effective (coarse mode) radius derived from AERONET inversions showed moderate but significant correlations. Correlations between coarse mode effective radius derived from alpha(c) (1.64 mu m) and surface-based volume mean diameter estimates underscored the physical significance of the spectral retrievals and suggested moderate vertical homogeneity in terms of coarse mode particle size. C1 [O'Neill, N. T.; Pancrati, O.] Univ Sherbrooke, CARTEL, Sherbrooke, PQ J1K 2R1, Canada. [Eck, T. F.; Smirnov, A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Reid, J. S.] Naval Res Lab, Monterey, CA 93943 USA. [Eck, T. F.; Smirnov, A.] Univ Maryland Baltimore Cty, Goddard Earth Sci & Technol Ctr, Baltimore, MD 21228 USA. RP O'Neill, NT (reprint author), Univ Sherbrooke, CARTEL, Sherbrooke, PQ J1K 2R1, Canada. EM norm.oneill@usherbrooke.ca RI ECK, THOMAS/D-7407-2012; Smirnov, Alexander/C-2121-2009; Reid, Jeffrey/B-7633-2014 OI Smirnov, Alexander/0000-0002-8208-1304; Reid, Jeffrey/0000-0002-5147-7955 NR 10 TC 9 Z9 9 U1 0 U2 1 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X EI 2169-8996 J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD MAR 13 PY 2008 VL 113 IS D5 AR D05212 DI 10.1029/2007JD009052 PG 11 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 276TL UT WOS:000254165900004 ER PT J AU Vorotnikov, VS Smith, CW Hu, Q Szabo, A Skoug, RM Cohen, CMS AF Vorotnikov, Vasiliy S. Smith, Charles W. Hu, Qiang Szabo, Adam Skoug, Ruth M. Cohen, Christina M. S. TI Automated shock detection and analysis algorithm for space weather application SO SPACE WEATHER-THE INTERNATIONAL JOURNAL OF RESEARCH AND APPLICATIONS LA English DT Article ID ADVANCED COMPOSITION EXPLORER; RANKINE-HUGONIOT PROBLEM; RADIATION BELT FORMATION; INTERPLANETARY SHOCKS; MAGNETIC-FIELDS; WIND; ACCELERATION AB [1] Space weather applications have grown steadily as real-time data have become increasingly available. Numerous industrial applications have arisen with safeguarding of the power distribution grids being a particular interest. NASA uses short-term and long-term space weather predictions in its launch facilities. Researchers studying ionospheric, auroral, and magnetospheric disturbances use real-time space weather services to determine launch times. Commercial airlines, communication companies, and the military use space weather measurements to manage their resources and activities. As the effects of solar transients upon the Earth's environment and society grow with the increasing complexity of technology, better tools are needed to monitor and evaluate the characteristics of the incoming disturbances. A need is for automated shock detection and analysis methods that are applicable to in situ measurements upstream of the Earth. Such tools can provide advance warning of approaching disturbances that have significant space weather impacts. Knowledge of the shock strength and speed can also provide insight into the nature of the approaching solar transient prior to arrival at the magnetopause. We report on efforts to develop a tool that can find and analyze shocks in interplanetary plasma data without operator intervention. This method will run with sufficient speed to be a practical space weather tool providing useful shock information within 1 min of having the necessary data to ground. The ability to run without human intervention frees space weather operators to perform other vital services. We describe ways of handling upstream data that minimize the frequency of false positive alerts while providing the most complete description of approaching disturbances that is reasonably possible. C1 [Vorotnikov, Vasiliy S.] Univ New Hampshire, Dept Chem Engn, Durham, NH USA. [Hu, Qiang] Univ New Hampshire, Inst Geophys, Durham, NH USA. [Smith, Charles W.] Univ New Hampshire, Ctr Space Sci, Durham, NH 03824 USA. [Szabo, Adam] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Skoug, Ruth M.] Los Alamos Natl Lab, Los Alamos, NM USA. [Cohen, Christina M. S.] CALTECH, Space Radiat Lab, Pasadena, CA USA. RP Vorotnikov, VS (reprint author), Univ New Hampshire, Dept Chem Engn, Durham, NH USA. NR 39 TC 12 Z9 13 U1 0 U2 3 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 1542-7390 J9 SPACE WEATHER JI Space Weather PD MAR 13 PY 2008 VL 6 IS 3 AR S03002 DI 10.1029/2007SW000358 PG 12 WC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology & Atmospheric Sciences SC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology & Atmospheric Sciences GA 276UU UT WOS:000254169800001 ER PT J AU Taktakishvili, A Kuznetsova, MM Hesse, M Fok, MC Rastaetter, L Maddox, M Chulaki, A Toth, G Gombosi, TI De Zeeuw, DL AF Taktakishvili, A. Kuznetsova, M. M. Hesse, M. Fok, M. -C. Rastaetter, L. Maddox, M. Chulaki, A. Toth, G. Gombosi, T. I. De Zeeuw, D. L. TI Role of periodic loading-unloading in the magnetotail versus interplanetary magnetic field B(z) flipping in the ring current buildup SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article ID MODEL AB Introducing kinetic corrections into the to BATSRUS code in the magnetotail region leads to fast reconnection rates observed in kinetic simulations and quasi-periodic loading-unloading cycles in the magnetotail during a long period of steady southward interplanetary magnetic field (IMF) B(z) (Kuznetsova et al., 2006, 2007). We use the global MHD code BATSRUS output to drive the Fok Ring Current (FRC) model, which then exhibits quasi-periodic oscillations of geosynchronous energetic particle fluxes, similar to "sawtooth'' injection profiles. We compare these results with the results of the FRC model driven by BATSRUS for periodically flipping IMF Bz component, without kinetic corrections. The comparison shows the dominant role of quasi-periodic loading-unloading in the tail over the role of flipping IMF Bz component in the formation of geosynchronous fluxes for various energies. This same result is confirmed by the analysis of particle number and energy content within geosynchronous orbit. C1 [Taktakishvili, A.; Kuznetsova, M. M.; Hesse, M.; Fok, M. -C.; Rastaetter, L.; Maddox, M.; Chulaki, A.] NASA, Goddard Space Flight Ctr, Heliophys Sci Div, Greenbelt, MD 20771 USA. [Toth, G.; Gombosi, T. I.; De Zeeuw, D. L.] Univ Michigan, Ctr Space Environm Modeling, Ann Arbor, MI 48109 USA. RP Taktakishvili, A (reprint author), NASA, Goddard Space Flight Ctr, Heliophys Sci Div, Greenbelt, MD 20771 USA. EM staktak@lssp-mail.gsfc.nasa.gov RI Gombosi, Tamas/G-4238-2011; De Zeeuw, Darren/F-3667-2011; Hesse, Michael/D-2031-2012; Rastaetter, Lutz/D-4715-2012; Kuznetsova, Maria/F-6840-2012; Fok, Mei-Ching/D-1626-2012; Toth, Gabor/B-7977-2013 OI Gombosi, Tamas/0000-0001-9360-4951; Rastaetter, Lutz/0000-0002-7343-4147; Toth, Gabor/0000-0002-5654-9823 NR 12 TC 1 Z9 1 U1 0 U2 0 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0148-0227 J9 J GEOPHYS RES-SPACE JI J. Geophys. Res-Space Phys. PD MAR 12 PY 2008 VL 113 IS A3 AR A03206 DI 10.1029/2007JA012845 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 276UM UT WOS:000254168800003 ER PT J AU Quillen, AC Bland-Hawthorn, J Green, JD Smith, JD Prasad, DA Alonso-Herrero, A Cleary, K Brookes, MH Lawrence, CR AF Quillen, Alice C. Bland-Hawthorn, Joss Green, Joel D. Smith, J. D. Prasad, D. Amelia Alonso-Herrero, Almudena Cleary, Kieran Brookes, Mairi H. Lawrence, Charles R. TI Spitzer Space Telescope Infrared Spectrograph mapping of the central kpc of Centaurus A SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE ISM : jets and outflows; galaxies : individual : NGC 5128; galaxies : ISM; galaxies : jets; galaxies : nuclei; galaxies : structure ID WARM MOLECULAR-HYDROGEN; RADIO GALAXY CENTAURUS; X-RAY-EMISSION; SEYFERT-GALAXIES; INTERSTELLAR-MEDIUM; LINE DIAGNOSTICS; SPECTROSCOPY; NUCLEUS; GAS; KINEMATICS AB We report on the results of spectroscopic mapping observations carried out in the central kpc of Centaurus A (NGC 5128) over the 5.2-15 and 20-36 mu m spectral regions using the Infrared Spectrograph onboard the Spitzer Space Telescope. The 500-pc bipolar dust shell discovered by Quillen et al. is even more clearly seen in the 11.3-mu m dust emission feature than previous broad-band imaging. The pure rotational lines of molecular hydrogen other than the S(0) line are detected above the dusty disc and associated with the oval dust shell. The molecular hydrogen transitions indicate the presence of warm gas at temperatures 250-720 K. The ratio of the surface brightnesses in the dust emission features at 7.7 and 11.3 mu m and the ratio of the [Ne II](12.8 mu m) and 11.3-mu m dust emission feature are lower in the 500-pc dust shell than in the star-forming disc. The clearer shell morphology at 11.3 mu m, warm molecular hydrogen emission in the shell, and variation in line ratios in the shell compared to those in the disc, confirm spectroscopically that this shell is a separate coherent entity and is unlikely to be a chance superposition of dust filaments. The physical conditions in the shell are most similar to Galactic supernova remnants where blast waves encounter molecular clouds. The lines requiring the highest level of ionization, [Ne V](24.318 mu m) and [O IV](25.890 mu m), are detected 20-25 arcsec north-east and south-west of the nucleus and at position angles near the radio jet axis. Fine-structure line ratios and limits from this region suggest that the medium is a low-density one and illuminated by a hard radiation field at low ionization parameter. These higher S molecular hydrogen pure rotational transitions are also particularly bright in the same region as the [O IV] and [Ne V] emission. This suggests that the gas associated with the dust shell has been excited near the jet axis and is part of an ionization cone. C1 [Quillen, Alice C.; Green, Joel D.; Prasad, D. Amelia] Univ Rochester, Dept Phys & Astron, Rochester, NY 14627 USA. [Bland-Hawthorn, Joss] Anglo Australian Observ, Epping, NSW 2121, Australia. [Bland-Hawthorn, Joss] Univ Sydney, Sch Phys, Inst Astron, Sydney, NSW 2006, Australia. [Smith, J. D.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Alonso-Herrero, Almudena] CSIC, Inst Estructura Mat, Dept Astrofis Mol & Infrarroja, E-28006 Madrid, Spain. [Brookes, Mairi H.; Lawrence, Charles R.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Quillen, AC (reprint author), Univ Rochester, Dept Phys & Astron, Rochester, NY 14627 USA. EM aquillen@pas.rochester.edu; jbh@aao.gov.au; joel@pas.rochester.edu; jdsmith@as.arizona.edu; aalonso@damir.iem.csic.es RI Alonso-Herrero, Almudena/H-1426-2015 OI Alonso-Herrero, Almudena/0000-0001-6794-2519 NR 38 TC 9 Z9 9 U1 0 U2 1 PU BLACKWELL PUBLISHING PI OXFORD PA 9600 GARSINGTON RD, OXFORD OX4 2DQ, OXON, ENGLAND SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD MAR 11 PY 2008 VL 384 IS 4 BP 1469 EP 1482 DI 10.1111/j.1365-2966.2007.12768.x PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 270HK UT WOS:000253711700021 ER PT J AU Damineli, A Hillier, DJ Corcoran, MF Stahl, O Levenhagen, RS Leister, NV Groh, JH Teodoro, M Colombo, JFA Gonzalez, F Arias, J Levato, H Grosso, M Morrell, N Gamen, R Wallerstein, G Niemela, V AF Damineli, A. Hillier, D. J. Corcoran, M. F. Stahl, O. Levenhagen, R. S. Leister, N. V. Groh, J. H. Teodoro, M. Colombo, J. F. Albacete Gonzalez, F. Arias, J. Levato, H. Grosso, M. Morrell, N. Gamen, R. Wallerstein, G. Niemela, V. TI The periodicity of the eta Carinae events SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE stars : general; stars : individual : eta Carinae; stars : binary ID 2003.5 MINIMUM; HOMUNCULUS NEBULA; SPECTROSCOPY; VARIABILITY; INTERFEROMETRY; EMISSION; SPECTRA; BINARY; EJECTA AB Extensive spectral observations of eta Carinae over the last cycle, and particularly around the 2003.5 low-excitation event, have been obtained. The variability of both narrow and broad lines, when combined with data taken from two earlier cycles, reveal a common and well-defined period. We have combined the cycle lengths derived from the many lines in the optical spectrum with those from broad-band X-rays, optical and near-infrared observations, and obtained a period length of P-pres = 2022.7 +/- 1.3 d. Spectroscopic data collected during the last 60 yr yield an average period of P-avg = 2020 +/- 4 d, consistent with the present-day period. The period cannot have changed by more than Delta P/P = 0.0007 since 1948. This confirms the previous claims of a true, stable periodicity, and gives strong support to the binary scenario. We have used the disappearance of the narrow component of He I 6678 to define the epoch of the Cycle 11 minimum, T-0 = JD 245 2819.8. The next event is predicted to occur on 2009 January 11 (+/- 2 d). The dates for the start of the minimum in other spectral features and broad-bands are very close to this date, and have well-determined time-delays from the He I epoch. C1 [Damineli, A.; Levenhagen, R. S.; Leister, N. V.; Groh, J. H.; Teodoro, M.] Univ Sao Paulo, Inst Astron Geofis & Ciencias Atmosfericas, BR-05508900 Sao Paulo, Brazil. [Hillier, D. J.] Univ Pittsburgh, Dept Phys & Astron, Pittsburgh, PA 15260 USA. [Corcoran, M. F.] NASA, Goddard Space Flight Ctr, CRESST, Greenbelt, MD 20771 USA. [Corcoran, M. F.] NASA, Goddard Space Flight Ctr, Xray Astrophys Lab, Greenbelt, MD 20771 USA. [Corcoran, M. F.] Univ Space Res Assoc, Columbia, MD 21044 USA. [Stahl, O.] Univ Heidelberg, ZAH, D-69117 Heidelberg, Germany. [Colombo, J. F. Albacete] UNLP, FCAGLP, Buenos Aires, DF, Argentina. [Gonzalez, F.; Levato, H.; Grosso, M.; Gamen, R.] Complejo Astron El Leoncito, San Juan, Argentina. [Arias, J.] Univ La Serena, Dept Fis, La Serena, Chile. [Morrell, N.] Carnegie Observ, Las Campanas Observ, La Serena, Chile. [Wallerstein, G.] Univ Washington, Dept Astron, Seattle, WA 98195 USA. RP Damineli, A (reprint author), Univ Sao Paulo, Inst Astron Geofis & Ciencias Atmosfericas, Rua Matao 1226,Cidade Univ, BR-05508900 Sao Paulo, Brazil. EM damineli@astro.iag.usp.br RI Damineli, Augusto/D-8210-2012; Levenhagen, Ronaldo/A-1043-2008; Teodoro, Mairan/H-9123-2013; Gamen, Roberto/A-1728-2015 OI Damineli, Augusto/0000-0002-7978-2994; Levenhagen, Ronaldo/0000-0003-2499-9325; NR 33 TC 72 Z9 72 U1 0 U2 3 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD MAR 11 PY 2008 VL 384 IS 4 BP 1649 EP 1656 DI 10.1111/j.1365-2966.2007.12815.x PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 270HK UT WOS:000253711700038 ER PT J AU Shi, C Yan, H Gu, C Ghosh, D Seballos, L Chen, SW Zhang, JZ Chen, B AF Shi, Chao Yan, He Gu, Claire Ghosh, Debraj Seballos, Leo Chen, Shaowei Zhang, Jin Z. Chen, Bin TI A double substrate "sandwich" structure for fiber surface enhanced Raman scattering detection SO APPLIED PHYSICS LETTERS LA English DT Article ID OPTICAL-FIBER; SILVER; SPECTROSCOPY; PROBES; RESONANCE; SENSORS; TIPS AB A double substrate "sandwiching" structure has been designed and tested for molecular detection using surface enhanced Raman scattering (SERS). With silver (Ag) nanoparticles as SERS substrates and rhodamine 6G (R6G) as a test molecule, the results show that the "sandwich" configuration exhibits significantly higher SERS enhancement compared to just one of the substrates or a simple sum of the signals from the two separate substrates. The improved SERS sensitivity is attributed to a stronger electromagnetic field enhancement by the double substrate sandwich structure. (C) 2008 American Institute of Physics. C1 [Shi, Chao; Yan, He; Gu, Claire] Univ Calif Santa Cruz, Dept Elect Engn, Santa Cruz, CA 95064 USA. [Ghosh, Debraj; Seballos, Leo; Chen, Shaowei; Zhang, Jin Z.] Univ Calif Santa Cruz, Dept Chem & Biochem, Santa Cruz, CA 95064 USA. [Chen, Bin] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Gu, C (reprint author), Univ Calif Santa Cruz, Dept Elect Engn, Santa Cruz, CA 95064 USA. EM chaoshi@soe.ucsc.edu; claire@soe.ucsc.edu; zhang@chemistry.ucsc.edu RI Chen, Shaowei/B-5171-2013 OI Chen, Shaowei/0000-0002-3668-8551 NR 29 TC 35 Z9 37 U1 3 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 0003-6951 J9 APPL PHYS LETT JI Appl. Phys. Lett. PD MAR 10 PY 2008 VL 92 IS 10 AR 103107 DI 10.1063/1.2883957 PG 3 WC Physics, Applied SC Physics GA 274GH UT WOS:000253989300107 ER PT J AU Ackermann, M Adams, J Ahrens, J Andeen, K Auffenberg, J Bai, X Baret, B Barwick, SW Bay, R Beattie, K Becka, T Becker, JK Becker, KH Beimforde, M Berghaus, P Berley, D Bernardini, E Bertrand, D Besson, DZ Blaufuss, E Boersma, DJ Bohm, C Bolmont, J Boser, S Botner, O Bouchta, A Braun, J Burgess, T Castermans, T Chirkin, D Christy, B Clem, J Cowen, DF D'Agostino, MV Davour, A Day, CT De Clercq, C Demirors, L Descamps, F Desiati, P De Vries-Uiterweerd, G DeYoung, T Diaz-Velez, JC Dreyer, J Dumm, JP Duvoort, MR Edwards, WR Ehrlich, R Eisch, J Ellsworth, RW Evenson, PA Fadiran, O Fazely, AR Filimonov, K Finley, C Foerster, MM Fox, BD Franckowiak, A Franke, R Gaisser, TK Gallagher, J Ganugapati, R Geenen, H Gerhardt, L Goldschmidt, A Goodman, JA Gozzini, R Griesel, T Gross, A Grullon, S Gunasingha, RM Gurtner, M Ha, C Hallgren, A Halzen, F Han, K Hanson, K Hardtke, D Hardtke, R Hasegawa, Y Hauschildt, T Heise, J Helbing, K Hellwig, M Herquet, P Hill, GC Hodges, J Hoffman, KD Hommez, B Hoshina, K Hubert, D Hughey, B Hulss, JP Hulth, PO Hultqvist, K Hundertmark, S Inaba, M Ishihara, A Jacobsen, J Japaridze, GS Johansson, H Joseph, JM Kampert, KH Kappes, A Karg, T Karle, A Kawai, H Kelley, JL Kiryluk, J Kislat, F Kitamura, N Klein, SR Klepser, S Kohnen, G Kolanoski, H Kopke, L Kowalski, M Kowarik, T Krasberg, M Kuehn, K Kuwabara, T Labare, M Laihem, K Landsman, H Lauer, R Leich, H Leier, D Liubarsky, I Lundberg, J Lunemann, J Madsen, J Maruyama, R Mase, K Matis, HS McCauley, T McParland, CP Meagher, K Meli, A Messarius, T Meszaros, P Miyamoto, H Montaruli, T Morey, A Morse, R Movit, SM Muenich, K Nahnhauer, R Nam, JW Niessen, P Nygren, DR Olivas, A Ono, M Patton, S Heros, CPDL Piegsa, A Pieloth, D Pohl, AC Porrata, R Pretz, J Price, PB Przybylski, GT Rawlins, K Razzaque, S Redl, P Resconi, E Rhode, W Ribordy, M Rizzo, A Robbins, S Robbins, WJ Roth, P Rothmaier, F Rott, C Roucelle, C Rutledge, D Ryckbosch, D Sander, HG Sarkar, S Satalecka, K Schlenstedt, S Schmidt, T Schneider, D Schultz, O Seckel, D Semburg, B Seo, SH Sestayo, Y Seunarine, S Silvestri, A Smith, AJ Song, C Spiczak, GM Spiering, C Stamatikos, M Stanev, T Stezelberger, T Stokstad, RG Stoufer, MC Stoyanov, S Strahler, EA Straszheim, T Sulanke, KH Sullivan, GW Sumner, TJ Swillens, Q Taboada, I Tarasova, O Tepe, A Thollander, L Tilav, S Tluczykont, M Toale, PA Tosi, D Turcan, D Van Eijndhoven, N Vandenbroucke, J Van Overloop, A Viscomi, V Vogt, C Voigt, B Wagner, W Walck, C Waldmann, H Waldenmaier, T Walter, M Wang, YR Wendt, C Wiebusch, CH Wiedemann, C Wikstrom, G Williams, DR Wischnewski, R Wissing, H Woschnagg, K Xu, XW Yodh, G Yoshida, S Zornoza, JD AF Ackermann, M. Adams, J. Ahrens, J. Andeen, K. Auffenberg, J. Bai, X. Baret, B. Barwick, S. W. Bay, R. Beattie, K. Becka, T. Becker, J. K. Becker, K. -H. Beimforde, M. Berghaus, P. Berley, D. Bernardini, E. Bertrand, D. Besson, D. Z. Blaufuss, E. Boersma, D. J. Bohm, C. Bolmont, J. Boeser, S. Botner, O. Bouchta, A. Braun, J. Burgess, T. Castermans, T. Chirkin, D. Christy, B. Clem, J. Cowen, D. F. D'Agostino, M. V. Davour, A. Day, C. T. De Clercq, C. Demiroers, L. Descamps, F. Desiati, P. De Vries-Uiterweerd, G. DeYoung, T. Diaz-Velez, J. C. Dreyer, J. Dumm, J. P. Duvoort, M. R. Edwards, W. R. Ehrlich, R. Eisch, J. Ellsworth, R. W. Evenson, P. A. Fadiran, O. Fazely, A. R. Filimonov, K. Finley, C. Foerster, M. M. Fox, B. D. Franckowiak, A. Franke, R. Gaisser, T. K. Gallagher, J. Ganugapati, R. Geenen, H. Gerhardt, L. Goldschmidt, A. Goodman, J. A. Gozzini, R. Griesel, T. Gross, A. Grullon, S. Gunasingha, R. M. Gurtner, M. Ha, C. Hallgren, A. Halzen, F. Han, K. Hanson, K. Hardtke, D. Hardtke, R. Hasegawa, Y. Hauschildt, T. Heise, J. Helbing, K. Hellwig, M. Herquet, P. Hill, G. C. Hodges, J. Hoffman, K. D. Hommez, B. Hoshina, K. Hubert, D. Hughey, B. Huelss, J. -P. Hulth, P. O. Hultqvist, K. Hundertmark, S. Inaba, M. Ishihara, A. Jacobsen, J. Japaridze, G. S. Johansson, H. Joseph, J. M. Kampert, K. -H. Kappes, A. Karg, T. Karle, A. Kawai, H. Kelley, J. L. Kiryluk, J. Kislat, F. Kitamura, N. Klein, S. R. Klepser, S. Kohnen, G. Kolanoski, H. Koepke, L. Kowalski, M. Kowarik, T. Krasberg, M. Kuehn, K. Kuwabara, T. Labare, M. Laihem, K. Landsman, H. Lauer, R. Leich, H. Leier, D. Liubarsky, I. Lundberg, J. Luenemann, J. Madsen, J. Maruyama, R. Mase, K. Matis, H. S. McCauley, T. McParland, C. P. Meagher, K. Meli, A. Messarius, T. Meszaros, P. Miyamoto, H. Montaruli, T. Morey, A. Morse, R. Movit, S. M. Muenich, K. Nahnhauer, R. Nam, J. W. Niessen, P. Nygren, D. R. Olivas, A. Ono, M. Patton, S. Heros, C. Perez De Los Piegsa, A. Pieloth, D. Pohl, A. C. Porrata, R. Pretz, J. Price, P. B. Przybylski, G. T. Rawlins, K. Razzaque, S. Redl, P. Resconi, E. Rhode, W. Ribordy, M. Rizzo, A. Robbins, S. Robbins, W. J. Roth, P. Rothmaier, F. Rott, C. Roucelle, C. Rutledge, D. Ryckbosch, D. Sander, H. -G. Sarkar, S. Satalecka, K. Schlenstedt, S. Schmidt, T. Schneider, D. Schultz, O. Seckel, D. Semburg, B. Seo, S. H. Sestayo, Y. Seunarine, S. Silvestri, A. Smith, A. J. Song, C. Spiczak, G. M. Spiering, C. Stamatikos, M. Stanev, T. Stezelberger, T. Stokstad, R. G. Stoufer, M. C. Stoyanov, S. Strahler, E. A. Straszheim, T. Sulanke, K. -H. Sullivan, G. W. Sumner, T. J. Swillens, Q. Taboada, I. Tarasova, O. Tepe, A. Thollander, L. Tilav, S. Tluczykont, M. Toale, P. A. Tosi, D. Turcan, D. Van Eijndhoven, N. Vandenbroucke, J. Van Overloop, A. Viscomi, V. Vogt, C. Voigt, B. Wagner, W. Walck, C. Waldmann, H. Waldenmaier, T. Walter, M. Wang, Y. -R. Wendt, C. Wiebusch, C. H. Wiedemann, C. Wikstroem, G. Williams, D. R. Wischnewski, R. Wissing, H. Woschnagg, K. Xu, X. W. Yodh, G. Yoshida, S. Zornoza, J. D. CA IceCube Collaboration TI Search for ultra-high-energy neutrinos with amanda-II SO ASTROPHYSICAL JOURNAL LA English DT Article DE diffuse radiation; galaxies : active; neutrinos; telescopes ID COSMIC-RAYS; LIMITS; SELECTION; DETECTOR; FLUX; KNEE AB A search for diffuse neutrinos with energies in excess of 10(5) GeV is conducted with AMANDA-II data recorded between 2000 and 2002. Above 10(7) GeV, the Earth is essentially opaque to neutrinos. This fact, combined with the limited overburden of the AMANDA-II detector ( roughly 1.5 km), concentrates these ultra-high-energy neutrinos at the horizon. The primary background for this analysis is bundles of downgoing, high-energy muons from the interaction of cosmic rays in the atmosphere. No statistically significant excess above the expected background is seen in the data, and an upper limit is set on the diffuse all-flavor neutrino flux of E-2 Phi(90%CL) < 2.7x10(-7) GeV cm(-2) s(-1) sr(-1) valid over the energy range of 2x10(5) to 10(9) GeV. A number of models that predict neutrino fluxes from active galactic nuclei are excluded at the 90% confidence level. C1 [Barwick, S. W.; Gerhardt, L.; Silvestri, A.; Yodh, G.] Univ Calif Irvine, Dept Phys & Astron, Irvine, CA 92697 USA. [Adams, J.; Han, K.; Seunarine, S.] Univ Canterbury, Dept Phys & Astron, Christchurch 1, New Zealand. [Ahrens, J.; Gozzini, R.; Griesel, T.; Hellwig, M.; Koepke, L.; Kowarik, T.; Piegsa, A.; Rothmaier, F.; Sander, H. -G.] Johannes Gutenberg Univ Mainz, Inst Phys, D-55099 Mainz, Germany. [Andeen, K.; Becka, T.; Boersma, D. J.; Braun, J.; Desiati, P.; Diaz-Velez, J. C.; Dumm, J. P.; Eisch, J.; Finley, C.; Ganugapati, R.; Grullon, S.; Halzen, F.; Hanson, K.; Hill, G. C.; Hodges, J.; Hoshina, K.; Hughey, B.; Jacobsen, J.; Kappes, A.; Karle, A.; Kelley, J. L.; Kitamura, N.; Krasberg, M.; Landsman, H.; Maruyama, R.; Montaruli, T.; Morse, R.; Schneider, D.; Song, C.; Stamatikos, M.; Strahler, E. A.; Wang, Y. -R.; Wendt, C.; Zornoza, J. D.] Univ Wisconsin, Dept Phys, Madison, WI 53706 USA. [Auffenberg, J.; Becker, K. -H.; Franckowiak, A.; Geenen, H.; Gurtner, M.; Helbing, K.; Kampert, K. -H.; Karg, T.; Robbins, S.; Semburg, B.; Tepe, A.] Berg Univ Wuppertal, Dept Phys, D-42119 Wuppertal, Germany. [Bai, X.; Clem, J.; Demiroers, L.; Evenson, P. A.; Gaisser, T. K.; Hauschildt, T.; Kuwabara, T.; Niessen, P.; Seckel, D.; Stanev, T.; Stoyanov, S.; Tilav, S.; Waldenmaier, T.] Univ Delaware, Bartol Res Inst, Newark, DE 19716 USA. [Bai, X.; Demiroers, L.; Hauschildt, T.; Niessen, P.; Rizzo, A.; Stanev, T.; Stoyanov, S.; Waldenmaier, T.] Univ Delaware, Dept Phys & Astron, Newark, DE 19716 USA. [Baret, B.; De Clercq, C.; Hubert, D.; Kuehn, K.] Vrije Univ Brussels, Dienst ELEM, B-1050 Brussels, Belgium. [Bay, R.; D'Agostino, M. V.; Filimonov, K.; Hardtke, D.; Morey, A.; Porrata, R.; Price, P. B.; Taboada, I.; Vandenbroucke, J.; Woschnagg, K.] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA. [Beattie, K.; Chirkin, D.; Day, C. T.; Edwards, W. R.; Goldschmidt, A.; Joseph, J. M.; Kiryluk, J.; Klein, S. R.; Matis, H. S.; McCauley, T.; McParland, C. P.; Nygren, D. R.; Patton, S.; Przybylski, G. T.; Roucelle, C.; Stezelberger, T.; Stokstad, R. G.; Stoufer, M. C.] Lawrence Berkeley Natl Lab, Berkeley, CA 94720 USA. [Becker, J. K.; Dreyer, J.; Leier, D.; Luenemann, J.; Meli, A.; Messarius, T.; Muenich, K.; Rhode, W.] Univ Dortmund, Dept Phys, D-44221 Dortmund, Germany. [Beimforde, M.; Kislat, F.; Kolanoski, H.; Kowalski, M.] Humboldt Univ, Inst Phys, D-12489 Berlin, Germany. [Berghaus, P.; Bertrand, D.; Labare, M.; Swillens, Q.] Univ Libre Bruxelles, Fac Sci, B-1050 Brussels, Belgium. [Berley, D.; Blaufuss, E.; Christy, B.; Ehrlich, R.; Ellsworth, R. W.; Goodman, J. A.; Hoffman, K. D.; Meagher, K.; Olivas, A.; Pretz, J.; Redl, P.; Roth, P.; Schmidt, T.; Smith, A. J.; Straszheim, T.; Sullivan, G. W.; Turcan, D.] Univ Maryland, Dept Phys, College Pk, MD 20742 USA. [Besson, D. Z.] Univ Kansas, Dept Phys & Astron, Lawrence, KS 66045 USA. [Bohm, C.; Burgess, T.; Hulth, P. O.; Hultqvist, K.; Hundertmark, S.; Johansson, H.; Thollander, L.; Walck, C.; Wiedemann, C.; Wikstroem, G.] Stockholm Univ, Dept Phys, SE-10691 Stockholm, Sweden. [Botner, O.; Bouchta, A.; Davour, A.; Hallgren, A.; Lundberg, J.; Heros, C. Perez De Los; Pohl, A. C.] Uppsala Univ, Div High Energy Phys, S-75121 Uppsala, Sweden. [Castermans, T.; Herquet, P.; Kohnen, G.] Univ Mons, B-7000 Mons, Belgium. [Cowen, D. F.; DeYoung, T.; Foerster, M. M.; Fox, B. D.; Ha, C.; Meszaros, P.; Razzaque, S.; Robbins, W. J.; Rott, C.; Rutledge, D.; Seo, S. H.; Toale, P. A.; Viscomi, V.; Wagner, W.; Williams, D. R.] Penn State Univ, Dept Phys, University Pk, PA 16802 USA. [Cowen, D. F.; Meszaros, P.; Movit, S. M.; Razzaque, S.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Descamps, F.; Hommez, B.; Ryckbosch, D.; Van Overloop, A.] Univ Ghent, Dept Subatom & Radiat Phys, B-9000 Ghent, Belgium. [De Vries-Uiterweerd, G.; Duvoort, M. R.; Heise, J.; Van Eijndhoven, N.] Univ Utrecht, Dept Phys & Astron, SRON, NL-3584 CC Utrecht, Netherlands. [Fadiran, O.; Japaridze, G. S.] Clark Atlanta Univ, CTSPS, Atlanta, GA 30314 USA. [Fazely, A. R.; Gunasingha, R. M.; Xu, X. W.] So Univ, Dept Phys, Baton Rouge, LA 70813 USA. [Ackermann, M.; Bernardini, E.; Bolmont, J.; Boeser, S.; Franke, R.; Klepser, S.; Lauer, R.; Leich, H.; Nahnhauer, R.; Pieloth, D.; Satalecka, K.; Schlenstedt, S.; Spiering, C.; Sulanke, K. -H.; Tarasova, O.; Tluczykont, M.; Tosi, D.; Voigt, B.; Waldmann, H.; Walter, M.; Wischnewski, R.] DESY, D-15735 Zeuthen, Germany. [Gallagher, J.] Univ Wisconsin, Dept Astron, Madison, WI 53706 USA. [Gross, A.; Resconi, E.; Schultz, O.; Sestayo, Y.] Max Planck Inst Kernphys, D-69177 Heidelberg, Germany. [Hardtke, R.; Madsen, J.; Spiczak, G. M.] Univ Wisconsin, Dept Phys, River Falls, WI 54022 USA. [Hasegawa, Y.; Inaba, M.; Ishihara, A.; Kawai, H.; Mase, K.; Miyamoto, H.; Ono, M.; Yoshida, S.] Chiba Univ, Dept Phys, Chiba 2638522, Japan. [Huelss, J. -P.; Laihem, K.; Vogt, C.; Wiebusch, C. H.; Wissing, H.] Rhein Westfal TH Aachen, Inst Phys 3, D-52056 Aachen, Germany. [Liubarsky, I.; Sumner, T. J.] Univ London Imperial Coll Sci Technol & Med, Blackett Lab, London SW7 2BW, England. [Pohl, A. C.] Kalmar Univ, Sch Pure & Appl Nat Sci, S-39182 Kalmar, Sweden. [Rawlins, K.] Univ Alaska, Dept Phys & Astron, Anchorage, AK 99508 USA. [Ribordy, M.] Ecole Polytech Fed Lausanne, High Energy Phys Lab, CH-1015 Lausanne, Switzerland. [Sarkar, S.] Univ Oxford, Dept Phys, Oxford OX1 3NP, England. [Stamatikos, M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Zornoza, J. D.] Univ Valencia, CSIC, IFIC, Valencia 46071, Spain. RP Gerhardt, L (reprint author), Univ Calif Irvine, Dept Phys & Astron, Irvine, CA 92697 USA. EM gerhardt@hep.ps.uci.edu RI Zornoza, Juan de Dios/L-1604-2014; Maruyama, Reina/A-1064-2013; Song, Chihwa/A-3455-2008; Hundertmark, Stephan/A-6592-2010; Vogt, Christian/E-2028-2012; Wiebusch, Christopher/G-6490-2012; Kowalski, Marek/G-5546-2012; Hallgren, Allan/A-8963-2013; Botner, Olga/A-9110-2013; Tjus, Julia/G-8145-2012; Auffenberg, Jan/D-3954-2014; OI Zornoza, Juan de Dios/0000-0002-1834-0690; Maruyama, Reina/0000-0003-2794-512X; Perez de los Heros, Carlos/0000-0002-2084-5866; Wiebusch, Christopher/0000-0002-6418-3008; Auffenberg, Jan/0000-0002-1185-9094; Hubert, Daan/0000-0002-4365-865X; Lauer, Robert/0000-0003-1933-7861; Sarkar, Subir/0000-0002-3542-858X NR 56 TC 74 Z9 74 U1 1 U2 9 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 MAR 10 PY 2008 VL 675 IS 2 BP 1014 EP 1024 DI 10.1086/527046 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 271VT UT WOS:000253817500006 ER PT J AU Rykoff, ES Mckay, TA Becker, MR Evrard, A Johnston, DE Koester, BP Rozo, E Sheldon, ES Wechsler, RH AF Rykoff, E. S. McKay, T. A. Becker, M. R. Evrard, A. Johnston, D. E. Koester, B. P. Rozo, E. Sheldon, E. S. Wechsler, R. H. TI Measuring the mean and scatter of the X-ray luminosity-optical richness relation for maxBCG galaxy clusters SO ASTROPHYSICAL JOURNAL LA English DT Review DE galaxies : clusters : general; X-rays : galaxies : clusters ID DIGITAL SKY SURVEY; SPECTROSCOPIC TARGET SELECTION; WEAK-LENSING ANALYSIS; FLUX-LIMITED SAMPLE; SUNYAEV-ZELDOVICH; REDSHIFT SURVEY; ABELL CLUSTERS; DISTANT CLUSTERS; COOLING-CORE; DARK-MATTER AB Determining the scaling relations between galaxy cluster observables requires large samples of uniformly observed clusters. We measure the mean X-ray luminosity-optical richness ((L) over bar (X)-(N) over bar (200)) relation for an approximately volume-limited sample of more than 17,000 optically selected clusters from the maxBCG catalog spanning the redshift range 0.1 < z < 0.3. By stacking the X-ray emission from many clusters using ROSAT All-Sky Survey data, we are able to measure mean X-ray luminosities to similar to 10% (including systematic errors) for clusters in nine independent optical richness bins. In addition, we are able to crudely measure individual X-ray emission from similar to 800 of the richest clusters. Assuming a lognormal form for the scatter in the L-X-N-200 relation, we measure sigma(ln L) = 0.86 +/- 0.03 at fixed N-200. This scatter is large enough to significantly bias the mean stacked relation. The corrected median relation can be parameterized by (L) over tilde (X) = e(alpha)((N) over bar (200)/40)(beta) x 10(42) h(-2) ergs s(-1), where alpha = 3.57 +/- 0.08 and beta = 1.82 +/- 0.05. We find that X-ray-selected clusters are significantly brighter than optically selected clusters at a given optical richness. This selection bias explains the apparently X-ray-underluminous nature of optically selected cluster catalogs. C1 [Rykoff, E. S.] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA. [Rykoff, E. S.; McKay, T. A.; Becker, M. R.; Evrard, A.] Univ Michigan, Dept Phys, Ann Arbor, MI 48109 USA. [McKay, T. A.; Evrard, A.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [McKay, T. A.; Evrard, A.] Michigan Ctr Theoret Phys, Ann Arbor, MI 48109 USA. [Johnston, D. E.] Jet Prop Lab, Pasadena, CA 91109 USA. [Koester, B. P.] Univ Chicago, Dept Astron, Chicago, IL 60637 USA. [Rozo, E.] Ohio State Univ, Columbus, OH 43201 USA. [Sheldon, E. S.] NYU, Dept Phys, Ctr Cosmol & Particle Phys, New York, NY 10003 USA. [Wechsler, R. H.] Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, Dept Phys, Stanford, CA 94305 USA. [Wechsler, R. H.] Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, Stanford Linear Accelerator Ctr, Stanford, CA 94305 USA. RP Rykoff, ES (reprint author), Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA. EM erykoff@physics.ucsb.edu RI McKay, Timothy/C-1501-2009; OI McKay, Timothy/0000-0001-9036-6150; Evrard, August/0000-0002-4876-956X; Becker, Matthew/0000-0001-7774-2246 NR 106 TC 58 Z9 58 U1 0 U2 1 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 MAR 10 PY 2008 VL 675 IS 2 BP 1106 EP 1124 DI 10.1086/527537 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 271VT UT WOS:000253817500014 ER PT J AU Corbet, RHD Sokoloski, JL Mukai, K Markwardt, CB Tueller, J AF Corbet, R. H. D. Sokoloski, J. L. Mukai, K. Markwardt, C. B. Tueller, J. TI A comparison of the variability of the symbiotic X-ray binaries GX 1+4, 4U 1954+31, and 4U 1700+24 from Swift bat and RXTE ASM observations SO ASTROPHYSICAL JOURNAL LA English DT Article DE binaries : symbiotic; stars : individual (GX 1+4, 4U 1954+31, 4U 1700+24) stars : neutron; X-rays : binaries ID ACCRETING PULSAR GX-1+4; ALL-SKY MONITOR; NEUTRON-STAR; TIMING-EXPLORER; ORBITAL PERIOD; 2S 0114+650; SCUTUM X-1; RED NOISE; COUNTERPARTS; LUMINOSITY AB We present an analysis of the X-ray variability of three symbiotic X-ray binaries, GX 1+4, 4U 1700+24, and 4U 1954+31, using observations made with the Swift Burst Alert Telescope (BAT) and the Rossi X-Ray Timing Explorer (RXTE) All-Sky Monitor (ASM). Observations of 4U 1954+31 with the Swift BAT show modulation at a period near 5 hr. Models to explain this modulation are discussed, including the presence of an exceptionally slow X-ray pulsar in the system and accretion instabilities. We conclude that the most likely interpretation is that 4U 1954+31 contains one of the slowest known X-ray pulsars. Unlike 4U 1954+31, neither GX 1+4 nor 4U 1700+24 show any evidence for modulation on a timescale of hours. An analysis of the RXTE ASM light curves of GX 1+4, 4U 1700+24, and 4U 1954+31 does not show the presence of periodic modulation in any source, with the exception of a possible detection of the 5 hr period in 4U 1954+31, although there is considerable variability on long timescales for all three sources. There is no modulation in GX 1+4 on either the optical 1161 day orbital period or a previously reported 304 day X-ray period. For 4U 1700+24 we do not confirm the 404 day X-ray period previously proposed for this source from a shorter duration ASM light curve. We conclude that all three sources have substantial low-frequency noise in their power spectra that may give the appearance of periodic modulation if this noise is not properly accounted for, particularly if short-duration light curves are examined. C1 [Corbet, R. H. D.; Mukai, K.; Markwardt, C. B.] NASA, Goddard Space Flight Ctr, Xray Astrophys Lab, Greenbelt, MD 20771 USA. [Corbet, R. H. D.; Mukai, K.] Univ Maryland Baltimore Cty, CRESST, Baltimore, MD 21228 USA. [Sokoloski, J. L.] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA. [Markwardt, C. B.] Univ Maryland, Dept Astron, CRESST, College Pk, MD 20742 USA. [Tueller, J.] NASA, Goddard Space Flight Ctr, Astrophys Phys Lab, Greenbelt, MD 20771 USA. RP Corbet, RHD (reprint author), NASA, Goddard Space Flight Ctr, Xray Astrophys Lab, Mail Code 662, Greenbelt, MD 20771 USA. EM Corbet@nasa.gov RI Tueller, Jack/D-5334-2012 NR 57 TC 25 Z9 26 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 MAR 10 PY 2008 VL 675 IS 2 BP 1424 EP 1435 DI 10.1086/526337 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 271VT UT WOS:000253817500033 ER PT J AU Hartman, JM Patruno, A Chakrabarty, D Kaplan, DL Markwardt, CB Morgan, EH Ray, PS van der Klis, M Wijnands, R AF Hartman, Jacob M. Patruno, Alessandro Chakrabarty, Deepto Kaplan, David L. Markwardt, Craig B. Morgan, Edward H. Ray, Paul S. van der Klis, Michiel Wijnands, Rudy TI The long-term evolution of the spin, pulse shape, and orbit of the accretion-powered millisecond pulsar SAX J1808.4-3658 SO ASTROPHYSICAL JOURNAL LA English DT Article DE stars : individual (SAX J1808.4-3658); stars : neutron; X-rays : stars ID RAY-TIMING-EXPLORER; PROPORTIONAL COUNTER ARRAY; ACTIVE RADIO PULSAR; BINARY PSR B1957+20; NEUTRON-STARS; OPTICAL COUNTERPART; GRAVITATIONAL-RADIATION; CATACLYSMIC VARIABLES; IGR J00291+5934; EMISSION AB We present a 7 yr timing study of the 2.5 ms X-ray pulsar SAX J1808.4-3658, an X-ray transient with a recurrence time of approximate to 2 yr, using data from the Rossi X-Ray Timing Explorer covering four transient outbursts (1998-2005). We verify that the 401 Hz pulsation traces the spin frequency fundamental and not a harmonic. Substantial pulse shape variability, both stochastic and systematic, was observed during each outburst. Analysis of the systematic pulse shape changes suggests that, as an outburst dims, the X-ray "hot spot'' on the pulsar surface drifts longitudinally and a second hot spot may appear. The overall pulse shape variability limits the ability to measure spin frequency evolution within a given X-ray outburst (and calls previous. (nu) over dot measurements of this source into question), with typical upper limits of vertical bar(nu) over dot vertical bar less than or similar to 2.5 x 10(-14) Hz s(-1) (2 sigma). However, combining data from all the outbursts shows with high (6 sigma) significance that the pulsar is undergoing long-term spin down at a rate. (nu) over dot = (-5.6 +/- 2.0) x 10(-16) Hz s(-1), with most of the spin evolution occurring during X-ray quiescence. We discuss the possible contributions of magnetic propeller torques, magnetic dipole radiation, and gravitational radiation to the measured spin down, setting an upper limit of B < 1.5 x 10(8) G for the pulsar's surface dipole magnetic field and Q/I < 5 x 10(-9) for the fractional mass quadrupole moment. We also measured an orbital period derivative of (P) over dot(orb) (3.5 +/- 0.2) x 10(-12) s s(-1). This surprisingly large (P) over dot(orb) is reminiscent of the large and quasi-cyclic orbital period variation observed in the so-called black widow millisecond radio pulsars, which further strengthens previous speculation that SAX J1808.4-3658 may turn on as a radio pulsar during quiescence. In an appendix we derive an improved (0: 1500) source position from optical data. C1 MIT, Dept Phys, Cambridge, MA 02139 USA. MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1098 SJ Amsterdam, Netherlands. Univ Amsterdam, Ctr High Energy Astrophys, NL-1098 SJ Amsterdam, Netherlands. [Markwardt, Craig B.] Univ Maryland, Dept Astron, CRESST, College Pk, MD 20742 USA. [Markwardt, Craig B.] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA. [Ray, Paul S.] USN, Res Lab, Div Space Sci, Washington, DC 20375 USA. RP Hartman, JM (reprint author), MIT, Dept Phys, Cambridge, MA 02139 USA. EM jhartman@space.mit.edu; apatruno@science.uva.nl; deepto@space.mit.edu; craigm@milkyway.gsfc.nasa.gov; ehm@space.mit.edu; paul.ray@nrl.navy.mil; michiel@science.uva.nl; rudy@science.uva.nl OI Ray, Paul/0000-0002-5297-5278 NR 83 TC 104 Z9 104 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD MAR 10 PY 2008 VL 675 IS 2 BP 1468 EP 1486 DI 10.1086/527461 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 271VT UT WOS:000253817500037 ER PT J AU Suchy, S Pottschmidt, K Wilms, J Kreykenbohm, I Schonherr, G Kretschmar, P McBride, V Caballero, I Rothschild, RE Grinberg, V AF Suchy, Slawomir Pottschmidt, Katja Wilms, Joern Kreykenbohm, Ingo Schoenherr, Gabriele Kretschmar, Peter McBride, Vanessa Caballero, Isabel Rothschild, Richard E. Grinberg, Victoria TI Pulse phase-resolved analysis of the high-mass X-ray binary centaurus X-3 over two binary orbits SO ASTROPHYSICAL JOURNAL LA English DT Article DE pulsars : individual (Centarus X-3); stars : magnetic fields; X-rays : binaries; X-rays : stars ID CYCLOTRON-LINE FEATURES; STELLAR WIND ACCRETION; TIMING-EXPLORER; VELA X-1; CEN X-3; SCATTERING FEATURE; MAGNETIC-FIELDS; NEUTRON-STAR; DISCOVERY; SPECTRUM AB We present a detailed analysis of observations of the high-mass X-ray binary Cen X-3, spanning two consecutive binary orbits performed with the RXTE satellite in early March 1997. During this time Cen X-3 had a luminosity of L2-10 keV similar to (4-5) x 10(37) ergs s(-1) and a pulse period of 4.814 s. The PCA and HEXTE light curves both show a clear reduction in count rate after midorbit for both binary revolutions. We therefore analyze two broadband spectra for each orbit, before and after midorbit. Consistent with earlier observations, these four joint PCA and HEXTE spectra can be well described using a phenomenological pulsar continuum model, including an iron emission line and a cyclotron resonance-scattering feature. While no strong spectral variations were detected, the second half of orbit 2 shows a tendency toward being softer and more strongly absorbed. In order to follow the orbital phase-dependent evolution of the spectrum in greater detail, we model spectra for shorter exposures, confirming that most spectral parameters show either a gradual or sudden change for the second half of the second orbit. A comparison with a simple wind model indicates the existence of an accretion wake in this system. We also present and discuss high-resolution pulse profiles for several different energy bands, as well as their hardness ratios. PCA and HEXTE spectra were created for 24 phase bins and fitted using the same model as in the phase-averaged case. Systematic pulse phase-dependent variations of several continuum and cyclotron line parameters were detected, most notably a significant increase of the cyclotron line energy during the early rise of the main peak, followed by a gradual decrease. We show that applying a simple dipole model for the magnetic field is not sufficient to describe our data. C1 [Suchy, Slawomir; Pottschmidt, Katja; Rothschild, Richard E.] Univ Calif San Diego, Ctr Astrophys & Space Sci, La Jolla, CA 92093 USA. [Pottschmidt, Katja] Univ Maryland Baltimore Cty, Dept Phys, Baltimore, MD 21250 USA. [Pottschmidt, Katja] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA. [Wilms, Joern] Astron Inst, D-96049 Bamberg, Germany. [Kreykenbohm, Ingo; Caballero, Isabel] Inst Astron & Astrophys, Abt Astron, D-72076 Tubingen, Germany. [Kreykenbohm, Ingo] INTEGRAL Sci Data Ctr, CH-1290 Versoix, Switzerland. [Schoenherr, Gabriele] Inst Astrophys, D-14482 Potsdam, Germany. [Kretschmar, Peter] European Space Agcy, European Space Astron Ctr, Madrid 28691, Spain. [McBride, Vanessa] Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England. [Grinberg, Victoria] Univ Munich, Fac Phys, D-80799 Munich, Germany. RP Suchy, S (reprint author), Univ Calif San Diego, Ctr Astrophys & Space Sci, 9500 Gilman Dr, La Jolla, CA 92093 USA. EM ssuchy@ucsd.edu; kpottschmidt@ucsd.edu; joern.wilms@sternwarte.uni-erlangen.de; kreyken@astro.uni-tuebingen.de; gschoenherr@aip.de; peter.kretschmar@esa.int; vanessa@astro.soton.ac.uk; isabel@astro.uni-tuebingende; rrothschild@ucsd.edu; victoria.grinberg@physik.lmu.de RI Wilms, Joern/C-8116-2013; Kreykenbohm, Ingo/H-9659-2013; OI Wilms, Joern/0000-0003-2065-5410; Kreykenbohm, Ingo/0000-0001-7335-1803; Kretschmar, Peter/0000-0001-9840-2048 NR 64 TC 34 Z9 34 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 MAR 10 PY 2008 VL 675 IS 2 BP 1487 EP 1498 DI 10.1086/527042 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 271VT UT WOS:000253817500038 ER PT J AU Thommes, EW Bryden, G Wu, YQ Rasio, FA AF Thommes, Edward W. Bryden, Geoffrey Wu, Yanqin Rasio, Frederic A. TI From mean motion resonances to scattered planets: Producing the solar system, eccentric exoplanets, and late heavy bombardments SO ASTROPHYSICAL JOURNAL LA English DT Article DE planetary systems : formation; solar system : formation ID EDGEWORTH-KUIPER BELT; GIANT PLANETS; PROTOPLANETARY DISK; DYNAMICAL INSTABILITIES; PLANETESIMAL DISK; ORBITAL EVOLUTION; DENSITY WAVES; MIGRATION; NEPTUNE; ORIGIN AB We show that interaction with a gas disk may produce young planetary systems with closely spaced orbits, stabilized by mean motion resonances between neighbors. On longer timescales, after the gas is gone, interaction with a remnant planetesimal disk tends to pull these configurations apart, eventually inducing dynamical instability. We find that this can lead to a variety of outcomes; some cases resemble the solar system, while others end up with high-eccentricity orbits reminiscent of the observed exoplanets. A similar mechanism has been previously suggested as the cause of the lunar late heavy bombardment. Thus, it may be that a large-scale dynamical instability, with more or less cataclysmic results, is an evolutionary step common to many planetary systems, including our own. C1 [Thommes, Edward W.; Rasio, Frederic A.] Northwestern Univ, Dept Phys & Astron, Evanston, IL 60208 USA. [Bryden, Geoffrey] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Wu, Yanqin] Univ Toronto, Dept Astron & Astrophys, Toronto, ON M5S 3H4, Canada. RP Thommes, EW (reprint author), Northwestern Univ, Dept Phys & Astron, Evanston, IL 60208 USA. OI Rasio, Frederic/0000-0002-7132-418X NR 46 TC 43 Z9 43 U1 1 U2 6 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 MAR 10 PY 2008 VL 675 IS 2 BP 1538 EP 1548 DI 10.1086/525244 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 271VT UT WOS:000253817500044 ER PT J AU Atrio-Barandela, F Kashlinsky, A Kocevski, D Ebeling, H AF Atrio-Barandela, F. Kashlinsky, A. Kocevski, D. Ebeling, H. TI Measurement of the electron-pressure profile of galaxy clusters in 3 year Wilkinson microwave anisotropy probe (WMAP) data SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE cosmic microwave background; cosmology : observations; cosmology : theory ID X-RAY SEARCH; INTRACLUSTER MEDIUM; POWER SPECTRUM; MILKY-WAY; SAMPLE; MAPS; GAS; COSMOLOGY; EINSTEIN; DENSITY AB Using 3 year WMAP data at the locations of similar to 700 X-ray-selected clusters, we have detected the amplitude of the thermal Sunyaev-Zeldovich (TSZ) effect at the 15 sigma level, the highest statistical significance reported so far. Owing to the large size of our cluster sample, we are able to detect the corresponding cosmic microwave background distortions out to large cluster-centric radii. The region over which the TSZ signal is detected is, on average, 4 times larger in radius than the X-ray-emitting region, extending to similar to 3 h(70)(-1) Mpc. We show that an isothermal b- model does not fit the electron pressure at large radii; instead, the baryon profile is consistent with the Navarro-Frenk-White profile, which is expected for dark matter in the concordance Lambda CDM model. The Xray temperature at the virial radius of the clusters falls by a factor similar to 3-4 from the central value, depending on the cluster concentration parameter. Our results suggest that cluster dynamics at large radii is dominated by dark matter and is well described by Newtonian gravity. C1 [Atrio-Barandela, F.] Univ Salamanca, E-37008 Salamanca, Spain. [Kashlinsky, A.] NASA, Goddard Space Flight Ctr, SSAI, Greenbelt, MD 20771 USA. [Kashlinsky, A.] NASA, Goddard Space Flight Ctr, Observat Cosmol Lab, Greenbelt, MD 20771 USA. [Kocevski, D.] Univ Calif Davis, Dept Phys, Davis, CA 95616 USA. [Ebeling, H.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. RP Atrio-Barandela, F (reprint author), Univ Salamanca, E-37008 Salamanca, Spain. EM atrio@usal.es RI Atrio-Barandela, Fernando/A-7379-2017 OI Atrio-Barandela, Fernando/0000-0002-2130-2513 NR 37 TC 43 Z9 43 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD MAR 10 PY 2008 VL 675 IS 2 BP L57 EP L60 DI 10.1086/533437 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 291ZC UT WOS:000255235100001 ER PT J AU Nitta, NV Mason, GM Wiedenbeck, ME Cohen, CMS Krucker, S Hannah, IG Shimojo, M Shibata, K AF Nitta, Nariaki V. Mason, Glenn M. Wiedenbeck, Mark E. Cohen, Christina M. S. Krucker, Sam Hannah, Iain G. Shimojo, Masumi Shibata, Kazunari TI Coronal jet observed by Hinode as the source of a He-3-rich solar energetic particle event SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE Sun : flares; Sun : particle emission; Sun : X-rays; gamma rays ID X-RAY JETS; ISOTOPE SPECTROMETER; ELECTRON EVENTS; WIND SPACECRAFT; TELESCOPE; MISSION; PLASMA; IMAGER; SUN; ACCELERATION AB We study the solar source of the 3He-rich solar energetic particle (SEP) event observed on 2006 November 18. The SEP event showed a clear velocity dispersion at energies below 1 MeV nucleon(-1), indicating its solar origin. We associate the SEP event with a coronal jet in an active region at heliographic longitude of W50 degrees, as observed in soft X-rays. This jet was the only noticeable activity in full-disk X-ray images around the estimated release time of the ions. It was temporally correlated with a series of type III radio bursts detected in metric and longer wavelength ranges and was followed by a nonrelativistic electron event. The jet may be explained in terms of the model of an expanding loop reconnecting with a large-scale magnetic field, which is open to interplanetary space for the particles to be observed at 1 AU. The open field lines appear to be anchored at the boundary between the umbra and penumbra of the leading sunspot, where a brightening is observed in both soft and hard X-rays during the jet activity. Other flares in the same region possibly associated with He-3-rich SEP events were not accompanied by a jet, indicative of different origins of this type of SEP event. C1 [Nitta, Nariaki V.] Org ADBS, Lockheed Martin Solar & Astrophys Lab, Palo Alto, CA 94304 USA. [Mason, Glenn M.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA. [Wiedenbeck, Mark E.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Wiedenbeck, Mark E.; Cohen, Christina M. S.] CALTECH, Space Radiat Lab, Pasadena, CA 91125 USA. [Krucker, Sam; Hannah, Iain G.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Krucker, Sam; Shimojo, Masumi] Natl Inst Nat Sci, Natl Astron Observ Japan, Nobeyama Radio Observ, Minamimaki, Nagano 3841305, Japan. [Shibata, Kazunari] Kyoto Univ, Kwasan Observ, Yamashina Ku, Kyoto 6078471, Japan. [Shibata, Kazunari] Kyoto Univ, Hida Observ, Yamashina Ku, Kyoto 6078471, Japan. RP Nitta, NV (reprint author), Org ADBS, Lockheed Martin Solar & Astrophys Lab, Bldg 252,3251 Hanover St, Palo Alto, CA 94304 USA. EM nitta@lmsal.com RI Hannah, Iain/F-1972-2011; Shimojo, Masumi/J-2605-2016 OI Hannah, Iain/0000-0003-1193-8603; Shimojo, Masumi/0000-0002-2350-3749 NR 31 TC 24 Z9 24 U1 0 U2 6 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 EI 2041-8213 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD MAR 10 PY 2008 VL 675 IS 2 BP L125 EP L128 DI 10.1086/533438 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 291ZC UT WOS:000255235100018 ER PT J AU Remijan, AJ Hollis, JM Lovas, FJ Stork, WD Jewell, PR Meier, DS AF Remijan, Anthony J. Hollis, J. M. Lovas, F. J. Stork, Wilmer D. Jewell, P. R. Meier, D. S. TI Detection of interstellar cyanoformaldehyde (CNCHO) SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE ISM : abundances; ISM : clouds; ISM : individual (Sagittarius B2(N-LMH)); ISM : molecules; radio lines : ISM ID GREEN-BANK TELESCOPE; FORMYL CYANIDE; GALACTIC-CENTER; GLYCOLALDEHYDE; CHOCN; MOLECULES; SPECTRUM; SUGAR; LINES; HCOCN AB Cyanoformaldehyde (CNCHO) has been detected toward the star-forming region Sagittarius B-2(N) with the 100 m Green Bank Telescope (GBT) by means of four P-branch rotational transitions in emission, the 7(0, 7)-6(1, 6) at 8.6 GHz, the 8(0, 8)-7(1, 7) at 19.4 GHz, the 9(0, 9)-8(1, 8) at 30.3 GHz, and the 10(0, 10)-9(1, 9) at 41.3 GHz, and one P-branch transition in absorption, the 5(1, 5)-6(0, 6) at 2.1 GHz. The five b-type transitions have favorable transition line strengths (S-ij mu(2) > 10 D-2) and occur in spectral regions that have little possibility of confusion with other molecular 2 species. The transition line strengths and energy levels involved in the four cyanoformaldehyde transitions in emission are similar; however, transitions with larger beam sizes give systematically higher column densities, suggesting that CNCHO is spatially extended and not concentrated toward the Sgr B2(N-LMH) position. Moreover, with a GBT beamwidth of similar to 350'', the 5(1, 5)-6(0, 6) transition of CNCHO was detected in absorption, confirming the widespread spatial extent of this molecule. We suggest that cyanoformaldehyde is likely formed in a neutral-radical reaction of two other interstellar molecules known for widespread spatial distributions: formaldehyde (H2CO) and the cyanide (CN) radical. C1 [Remijan, Anthony J.; Jewell, P. R.] Natl Radio Astron Observ, Charlottesville, VA 22903 USA. [Hollis, J. M.] NASA, Goddard Space Flight Ctr, Computat & Informat Sci & Technol Off, Greenbelt, MD 20771 USA. [Lovas, F. J.] Natl Inst Stand & Technol, Opt Technol Div, Gaithersburg, MD 20899 USA. [Stork, Wilmer D.] Plastipak Packaging Inc, Champaign, IL 61821 USA. [Stork, Wilmer D.] Parkland Coll, Dept Nat Sci, Champaign, IL 61821 USA. [Meier, D. S.] Natl Radio Astron Observ, Socorro, NM 87801 USA. RP Remijan, AJ (reprint author), Natl Radio Astron Observ, 520 Edgemont Rd, Charlottesville, VA 22903 USA. NR 27 TC 23 Z9 23 U1 1 U2 4 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD MAR 10 PY 2008 VL 675 IS 2 BP L85 EP L88 DI 10.1086/533529 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 291ZC UT WOS:000255235100008 ER PT J AU Prates-Clark, CD Saatchi, SS Agosti, D AF Prates-Clark, Cassia Da Conceicao Saatchi, Sassan S. Agosti, Donat TI Predicting geographical distribution models of high-value timber trees in the Amazon Basin using remotely sensed data SO ECOLOGICAL MODELLING LA English DT Article DE Amazon Basin; climate variables; ecological niche; remote sensing data; species distribution model; timber trees ID GLOBAL LAND AREAS; RAIN-FOREST; VIROLA-SURINAMENSIS; SPECIES RICHNESS; BRAZILIAN AMAZON; PLANT-GROWTH; CORAL-REEFS; COSTA-RICA; LEAF-AREA; VEGETATION AB Species distribution models were developed for three high economic value timber trees (Calophyllum brasiliensis, Carapa quianensis and Virola surinamensis) that are heavily harvested in the Amazon Basin. A combination of habitat measurements extracted from remote sensing data (MODIS, QSCAT and SRTM) and bioclimatic surfaces was examined to ascertain the most influential factors determining the occurrence of these tree species. The prediction of species' occurrence rates was tested separately for each species distribution model and the results were examined for their ability to accurately map the spatial distribution of these tree species. By evaluating the omission and commission rates we concluded that species distribution models based on remote sensing data contributed significantly in quantifying environmental properties used to summarize the ecological niche of each tree species. Specific vegetation characteristics (such as percentage of tree cover, vegetation moisture and roughness, annual NDVI and mean LAI during the dry LAI) showed the dependence of these species' occurrence in more densely vegetated forests. Areas with high leaf area (even during the dry months) and areas with high vegetation moisture were predicted as potential species habitat for C. brasiliensis. The density vegetation during the dry season and vegetation phenology were strongly correlated with climate differences, such as variations in air temperature and precipitation seasonality for V surinamensis. Lower elevation areas with more exuberant vegetation and a high greenness index were among the most important factors accounting for the geographical distribution of C. guianensis. Species distribution models are increasingly important in many fields of research and conservation. The potential of remotely sensed data to monitor environmental changes in tropical areas, along with the understanding of ecosystem function, are both critical for conservation of biodiversity and the long-term process of sustaining ecosystems. (c) 2007 Elsevier B.V All rights reserved. C1 [Prates-Clark, Cassia Da Conceicao] Univ Bristol, Sch Geog Sci, Bristol BS8 1SS, Avon, England. [Prates-Clark, Cassia Da Conceicao; Saatchi, Sassan S.] Univ Calif Los Angeles, Ctr Trop Res, Los Angeles, CA 90095 USA. [Saatchi, Sassan S.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Agosti, Donat] Naturmuseum Burgergemeinde Bern, CH-3005 Bern, Switzerland. RP Prates-Clark, CD (reprint author), Univ Bristol, Sch Geog Sci, Univ Rd, Bristol BS8 1SS, Avon, England. EM Cassia.Prates-Clark@bristol.ac.uk OI Agosti, Donat /0000-0001-9286-1200 NR 91 TC 30 Z9 34 U1 1 U2 24 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0304-3800 EI 1872-7026 J9 ECOL MODEL JI Ecol. Model. PD MAR 10 PY 2008 VL 211 IS 3-4 BP 309 EP 323 DI 10.1016/j.ecolmodel.2007.09.024 PG 15 WC Ecology SC Environmental Sciences & Ecology GA 270DS UT WOS:000253700900006 ER PT J AU Mlynczak, MG Martin-Torres, FJ Mertens, CJ Marshall, BT Thompson, RE Kozyra, JU Remsberg, EE Gordley, LL Russell, JM Woods, T AF Mlynczak, Martin G. Martin-Torres, F. Javier Mertens, Christopher J. Marshall, B. Thomas Thompson, R. Earl Kozyra, Janet U. Remsberg, Ellis E. Gordley, Larry L. Russell, James M., III Woods, Thomas TI Solar-terrestrial coupling evidenced by periodic behavior in geomagnetic indexes and the infrared energy budget of the thermosphere SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID MESOSPHERE; ENERGETICS AB We examine time series of the daily global power (W) radiated by carbon dioxide (at 15 mm) and by nitric oxide (at 5.3 mu m) from the Earth's thermosphere between 100 km and 200 km altitude. Also examined is a time series of the daily absorbed solar ultraviolet power in the same altitude region in the wavelength span 0 to 175 nm. The infrared data are derived from the SABER instrument and the solar data are derived from the SEE instrument, both on the NASA TIMED satellite. The time series cover nearly 5 years from 2002 through 2006. The infrared and solar time series exhibit a decrease in radiated and absorbed power consistent with the declining phase of the current 11-year solar cycle. The infrared time series also exhibits high frequency variations that are not evident in the solar power time series. Spectral analysis shows a statistically significant 9-day periodicity in the infrared data but not in the solar data. A very strong 9-day periodicity is also found to exist in the time series of daily A(p) and K(p) geomagnetic indexes. These 9-day periodicities are linked to the recurrence of coronal holes on the Sun. These results demonstrate a direct coupling between the upper atmosphere of the Sun and the infrared energy budget of the thermosphere. C1 [Mlynczak, Martin G.; Mertens, Christopher J.; Remsberg, Ellis E.] NASA, Langley Res Ctr, Hampton, VA 23681 USA. [Martin-Torres, F. Javier] Analyt Serv & Mat Inc, Hampton, VA 23666 USA. [Marshall, B. Thomas; Thompson, R. Earl; Gordley, Larry L.] G&A Tech Software, Newport News, VA 23606 USA. [Kozyra, Janet U.] Univ Michigan, Ann Arbor, MI 48109 USA. [Russell, James M., III] Hampton Univ, Hampton, VA USA. [Woods, Thomas] Univ Colorado, Atmospher & Space Phys Lab, Boulder, CO 80309 USA. RP Mlynczak, MG (reprint author), NASA, Langley Res Ctr, Mail Stop 420, Hampton, VA 23681 USA. EM m.g.mlynczak@nasa.gov RI Mlynczak, Martin/K-3396-2012; Martin-Torres, Francisco Javier/G-6329-2015 OI Martin-Torres, Francisco Javier/0000-0001-6479-2236 NR 16 TC 63 Z9 63 U1 0 U2 3 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD MAR 8 PY 2008 VL 35 IS 5 AR L05808 DI 10.1029/2007GL032620 PG 5 WC Geosciences, Multidisciplinary SC Geology GA 276QA UT WOS:000254156000004 ER PT J AU Ren, XR Olson, JR Crawford, JH Brune, WH Mao, JQ Long, RB Chen, Z Chen, G Avery, MA Sachse, GW Barrick, JD Diskin, GS Huey, LG Fried, A Cohen, RC Heikes, B Wennberg, PO Singh, HB Blake, DR Shetter, RE AF Ren, Xinrong Olson, Jennifer R. Crawford, James H. Brune, William H. Mao, Jingqiu Long, Robert B. Chen, Zhong Chen, Gao Avery, Melody A. Sachse, Glen W. Barrick, John D. Diskin, Glenn S. Huey, L. Greg Fried, Alan Cohen, Ronald C. Heikes, Brian Wennberg, Paul O. Singh, Hanwant B. Blake, Donald R. Shetter, Richard E. TI HOx chemistry during INTEX-A 2004: Observation, model calculation, and comparison with previous studies SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID LASER-INDUCED FLUORESCENCE; PEM-TROPICS-B; UPPER TROPOSPHERE; OZONE PRODUCTION; BOUNDARY-LAYER; NITROUS-ACID; RURAL SITE; TRACE-P; OH; RADICALS AB OH and HO2 were measured with the Airborne Tropospheric Hydrogen Oxides Sensor (ATHOS) as part of a large measurement suite from the NASA DC-8 aircraft during the Intercontinental Chemical Transport Experiment-A ( INTEX-A). This mission, which was conducted mainly over North America and the western Atlantic Ocean in summer 2004, was an excellent test of atmospheric oxidation chemistry. The HOx results from INTEX-A are compared to those from previous campaigns and to results for other related measurements from INTEX-A. Throughout the troposphere, observed OH was generally 0.95 of modeled OH; below 8 km, observed HO2 was generally 1.20 of modeled HO2. This observed-to-modeled comparison is similar to that for TRACE-P, another midlatitude study for which the median observed-to-modeled ratio was 1.08 for OH and 1.34 for HO2, and to that for PEM-TB, a tropical study for which the median observed-to-modeled ratio was 1.17 for OH and 0.97 for HO2. HO2 behavior above 8 km was markedly different. The observed-to-modeled HO2 ratio increased from similar to 1.2 at 8 km to similar to 3 at 11 km with the observed-to-modeled ratio correlating with NO. Above 8 km, the observed-to-modeled HO2 and observed NO were both considerably greater than observations from previous campaigns. In addition, the observed-to-modeled HO2/OH, which is sensitive to cycling reactions between OH and HO2, increased from similar to 1.5 at 8 km to almost 3.5 at 11 km. These discrepancies suggest a large unknown HOx source and additional reactants that cycle HOx from OH to HO2. In the continental planetary boundary layer, the observed-to-modeled OH ratio increased from 1 when isoprene was less than 0.1 ppbv to over 4 when isoprene was greater than 2 ppbv, suggesting that forests throughout the United States are emitting unknown HOx sources. Progress in resolving these discrepancies requires a focused research activity devoted to further examination of possible unknown OH sinks and HOx sources. C1 [Ren, Xinrong; Brune, William H.; Mao, Jingqiu; Long, Robert B.; Chen, Zhong] Penn State Univ, Dept Meteorol, University Pk, PA 16802 USA. [Olson, Jennifer R.; Crawford, James H.; Chen, Gao; Avery, Melody A.; Sachse, Glen W.; Barrick, John D.; Diskin, Glenn S.] NASA, Langley Res Ctr, Sci Directorate, Hampton, VA 23681 USA. [Huey, L. Greg] Georgia Inst Technol, Sch Earth & Atmospher Sci, Atlanta, GA 30332 USA. [Fried, Alan] Natl Ctr Atmospher Res, Earth Observing Lab, Boulder, CO 80307 USA. [Cohen, Ronald C.] Univ Calif Berkeley, Dept Chem, Berkeley, CA 94720 USA. [Cohen, Ronald C.] Univ Calif Berkeley, Dept Earth & Planetary Sci, Berkeley, CA 94720 USA. [Heikes, Brian] Univ Rhode Isl, Grad Sch Oceanog, Kingston, RI 02881 USA. [Wennberg, Paul O.] CALTECH, Div Engn & Appl Sci, Pasadena, CA 91125 USA. [Singh, Hanwant B.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Blake, Donald R.] Univ Calif Irvine, Dept Chem, Irvine, CA 92697 USA. [Shetter, Richard E.] Univ N Dakota, Natl Suborbital Educ & Res Ctr, Grand Forks, ND 58202 USA. RP Ren, XR (reprint author), Univ Miami, Rosenstiel Sch Marine & Atmospher Sci, 4600 Rickenbacker Causeway, Miami, FL 33149 USA. EM xren@rsmas.miami.edu RI Mao, Jingqiu/F-2511-2010; Cohen, Ronald/A-8842-2011; Ren, Xinrong/B-2229-2010; Wennberg, Paul/A-5460-2012; Crawford, James/L-6632-2013; Ren, Xinrong/E-7838-2015 OI Mao, Jingqiu/0000-0002-4774-9751; Cohen, Ronald/0000-0001-6617-7691; Crawford, James/0000-0002-6982-0934; Ren, Xinrong/0000-0001-9974-1666 NR 42 TC 105 Z9 105 U1 2 U2 39 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X EI 2169-8996 J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD MAR 8 PY 2008 VL 113 IS D5 AR D05310 DI 10.1029/2007JD009166 PG 13 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 276QL UT WOS:000254157100006 ER PT J AU Kedar, S Longuet-Higgins, M Webb, F Graham, N Clayton, R Jones, C AF Kedar, Sharon Longuet-Higgins, Michael Webb, Frank Graham, Nicholas Clayton, Robert Jones, Cathleen TI The origin of deep ocean microseisms in the North Atlantic Ocean SO PROCEEDINGS OF THE ROYAL SOCIETY A-MATHEMATICAL PHYSICAL AND ENGINEERING SCIENCES LA English DT Article DE microseisms; wave-wave interaction; acoustic resonance; wave model; Stoneley waves ID RAYLEIGH-WAVE ATTENUATION; AMBIENT SEISMIC NOISE; SECONDARY MICROSEISMS; AMERICA; SEA; GENERATION; STATIONS; SPECTRUM AB Oceanic microseisms are small oscillations of the ground, in the frequency range of 0.05 0.3 Hz, associated with the occurrence of energetic ocean waves of half the corresponding frequency. In 1950, Longuet-Higgins suggested in a landmark theoretical paper that (i) microseisms originate from surface pressure oscillations caused by the interaction between oppositely travelling components with the same frequency in the ocean wave spectrum, (ii) these pressure oscillations generate seismic Stoneley waves on the ocean bottom, and (iii) when the ocean depth is comparable with the acoustic wavelength in water, compressibility must be considered. The efficiency of microseism generation thus depends on both the wave frequency and the depth of water. While the theory provided an estimate of the magnitude of the corresponding microseisms in a compressible ocean, its predictions of microseism amplitude heretofore have never been tested quantitatively. In this paper, we show a strong agreement between observed microseism and calculated amplitudes obtained by applying Longuet-Higgins' theory to hindcast ocean wave spectra from the North Atlantic Ocean. The calculated vertical displacements are compared with seismic data collected at stations in North America, Greenland, Iceland and Europe. This modelling identifies a particularly energetic source area stretching from the Labrador Sea to south of Iceland, where wind patterns are especially conducive to generating oppositely travelling waves of same period, and the ocean depth is favourable for efficient microseism generation through the 'organ pipe' resonance of the compression waves, as predicted by the theory. This correspondence between observations and the model predictions demonstrates that deep ocean nonlinear wave-wave interactions are sufficiently energetic to account for much of the observed seismic amplitudes in North America, Greenland and Iceland. C1 [Kedar, Sharon; Webb, Frank; Jones, Cathleen] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Longuet-Higgins, Michael] Univ Calif San Diego, Inst Nonlinear Sci, La Jolla, CA 92093 USA. [Clayton, Robert] CALTECH, Seismol Lab, Pasadena, CA 91125 USA. RP Kedar, S (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM sharon.kedar@jpl.nasa.gov RI GEOFON, GlobalSeismicNetwork/E-4273-2012 NR 39 TC 131 Z9 137 U1 2 U2 18 PU ROYAL SOC PI LONDON PA 6-9 CARLTON HOUSE TERRACE, LONDON SW1Y 5AG, ENGLAND SN 1364-5021 J9 P ROY SOC A-MATH PHY JI Proc. R. Soc. A-Math. Phys. Eng. Sci. PD MAR 8 PY 2008 VL 464 IS 2091 BP 777 EP 793 DI 10.1098/rspa.2007.0277 PG 17 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 256XM UT WOS:000252763200014 ER PT J AU Paillou, P Mitchell, K Wall, S Ruffie, G Wood, C Lorenz, R Stofan, E Lunine, J Lopes, R Encrenaz, P AF Paillou, Philippe Mitchell, Karl Wall, Stephen Ruffie, Gilles Wood, Charles Lorenz, Ralph Stofan, Ellen Lunine, Jonathan Lopes, Rosaly Encrenaz, Pierre TI Microwave dielectric constant of liquid hydrocarbons: Application to the depth estimation of Titan's lakes SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID CASSINI RADAR; SURFACE; MAPPER AB Cassini RADAR reveals the surface of Titan since flyby Ta acquired on October 2004. The RADAR instrument discovered volcanic structures, craters, dunes, channels, lakes and seas. In particular, flyby T16 realized in July 2006 imaged tens of radar-dark features close to Titan's north pole. They are interpreted as lakes filled with liquid hydrocarbons - mainly methane, a key material in the geologic and climatic history of Titan. In order to perform quantitative analysis and modeling of the radar response of Titan's lakes, the dielectric constant of liquid hydrocarbons is a crucial parameter, in particular to estimate the radar wave attenuation. We present here first measurements of the dielectric constant of LNG ( Liquefied Natural Gas), mainly composed of methane, at Ku-band ( 10 - 13 GHz): we obtained a value epsilon = 1.75 - 0.002j. This value is used to model the radar backscattering of lakes observed during T16 flyby. Using a two-layer scattering model, we derive a relationship that is used to estimate a minimum depth for Titan's lakes. The proposed relationship is also coherent with the observation that the larger and then the deeper lakes are also the darker in radar images. C1 [Paillou, Philippe] OASU, UMR 5804, F-33270 Floirac, France. [Encrenaz, Pierre] LERMA, Observ Paris, F-75014 Paris, France. [Mitchell, Karl; Wall, Stephen; Lopes, Rosaly] JPL, Pasadena, CA 91109 USA. [Lorenz, Ralph] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA. [Lunine, Jonathan] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA. [Ruffie, Gilles] IMS, UMR 5218, F-33607 Pessac, France. [Stofan, Ellen] Proxemy Res, Rectortown, VA 20140 USA. [Wood, Charles] Planetary Sci Inst, Tucson, AZ 85719 USA. RP Paillou, P (reprint author), OASU, UMR 5804, F-33270 Floirac, France. RI Lorenz, Ralph/B-8759-2016; Lopes, Rosaly/D-1608-2016 OI Lorenz, Ralph/0000-0001-8528-4644; Lopes, Rosaly/0000-0002-7928-3167 NR 25 TC 26 Z9 26 U1 1 U2 2 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 EI 1944-8007 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD MAR 7 PY 2008 VL 35 IS 5 AR L05202 DI 10.1029/2007GL032515 PG 5 WC Geosciences, Multidisciplinary SC Geology GA 276PZ UT WOS:000254155900003 ER PT J AU Anderson, JD Campbell, JK Ekelund, JE Ellis, J Jordan, JF AF Anderson, John D. Campbell, James K. Ekelund, John E. Ellis, Jordan Jordan, James F. TI Anomalous orbital-energy changes observed during spacecraft flybys of Earth SO PHYSICAL REVIEW LETTERS LA English DT Article ID GALILEO; SYSTEM AB We report and characterize anomalous orbital-energy changes observed during six Earth flybys by the Galileo, NEAR, Cassini, Rosetta, and MESSENGER spacecraft. These anomalous energy changes are consistent with an empirical prediction formula which is proportional to the total orbital energy per unit mass and which involves the incoming and outgoing geocentric latitudes of the asymptotic spacecraft velocity vectors. We use this formula to predict a potentially detectable flyby velocity increase of less than 1 mm/s for a second Rosetta flyby on November 13, 2007. C1 [Anderson, John D.; Campbell, James K.; Ekelund, John E.; Ellis, Jordan; Jordan, James F.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Anderson, JD (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. NR 15 TC 78 Z9 78 U1 1 U2 2 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 0031-9007 J9 PHYS REV LETT JI Phys. Rev. Lett. PD MAR 7 PY 2008 VL 100 IS 9 AR 091102 DI 10.1103/PhysRevLett.100.091102 PG 4 WC Physics, Multidisciplinary SC Physics GA 271BS UT WOS:000253764500011 PM 18352689 ER PT J AU Jones, GH Roussos, E Krupp, N Beckmann, U Coates, AJ Crary, F Dandouras, I Dikarev, V Dougherty, MK Garnier, P Hansen, CJ Hendrix, AR Hospodarsky, GB Johnson, RE Kempf, S Khurana, KK Krimigis, SM Kruger, H Kurth, WS Lagg, A McAndrews, HJ Mitchell, DG Paranicas, C Postberg, F Russell, CT Saur, J Seiss, M Spahn, F Srama, R Strobel, DF Tokar, R Wahlund, JE Wilson, RJ Woch, J Young, D AF Jones, G. H. Roussos, E. Krupp, N. Beckmann, U. Coates, A. J. Crary, F. Dandouras, I. Dikarev, V. Dougherty, M. K. Garnier, P. Hansen, C. J. Hendrix, A. R. Hospodarsky, G. B. Johnson, R. E. Kempf, S. Khurana, K. K. Krimigis, S. M. Krueger, H. Kurth, W. S. Lagg, A. McAndrews, H. J. Mitchell, D. G. Paranicas, C. Postberg, F. Russell, C. T. Saur, J. Seiss, M. Spahn, F. Srama, R. Strobel, D. F. Tokar, R. Wahlund, J. -E. Wilson, R. J. Woch, J. Young, D. TI The dust halo of Saturn's largest icy moon, Rhea SO SCIENCE LA English DT Article ID PLANETARY SATELLITES; CASSINI; MAGNETOSPHERE; CLOUDS AB Saturn's moon Rhea had been considered massive enough to retain a thin, externally generated atmosphere capable of locally affecting Saturn's magnetosphere. The Cassini spacecraft's in situ observations reveal that energetic electrons are depleted in the moon's vicinity. The absence of a substantial exosphere implies that Rhea's magnetospheric interaction region, rather than being exclusively induced by sputtered gas and its products, likely contains solid material that can absorb magnetospheric particles. Combined observations from several instruments suggest that this material is in the form of grains and boulders up to several decimetres in size and orbits Rhea as an equatorial debris disk. Within this disk may reside denser, discrete rings or arcs of material. C1 [Jones, G. H.; Roussos, E.; Krupp, N.; Dikarev, V.; Krueger, H.; Lagg, A.; Woch, J.] Max Planck Inst Sonnensystemforsch, D-37191 Katlenburg Lindau, Germany. [Jones, G. H.; Coates, A. J.; McAndrews, H. J.] UCL, Mullard Space Sci Lab, Dept Space & Climate Phys, Dorking RH5 6NT, Surrey, England. [Jones, G. H.; Coates, A. J.] UCL, Ctr Planetary Sci, London WC1E 6BT, England. [Beckmann, U.; Dikarev, V.; Kempf, S.; Postberg, F.; Srama, R.] Max Planck Inst Kernphys, D-69117 Heidelberg, Germany. [Crary, F.; Young, D.] SW Res Inst, San Antonio, TX 78238 USA. [Dandouras, I.; Garnier, P.] Univ Toulouse 3, CNRS, Ctr Etud Spatiale Rayonnements, F-31400 Toulouse, France. [Dikarev, V.] St Petersburg State Univ, Inst Astron, St Petersburg 198504, Russia. [Dougherty, M. K.] Univ London Imperial Coll Sci Technol & Med, Blackett Lab, London SW7 2BW, England. [Garnier, P.; Wahlund, J. -E.] Swedish Inst Space Phys, S-75121 Uppsala, Sweden. [Hansen, C. J.; Hendrix, A. R.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Hospodarsky, G. B.; Kurth, W. S.] Univ Iowa, Dept Phys & Astron, Iowa City, IA 52242 USA. [Johnson, R. E.] Univ Virginia, Dept Mat Sci & Engn, Charlottesville, VA 22904 USA. [Khurana, K. K.; Russell, C. T.] Univ Calif Los Angeles, Inst Geophys & Planetary Phys, Los Angeles, CA 90095 USA. [Krimigis, S. M.; Mitchell, D. G.; Paranicas, C.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA. [Krimigis, S. M.] Acad Athens, Athens 11527, Greece. [Saur, J.] Univ Cologne, Inst Geophys & Meteorol, D-50923 Cologne, Germany. [Seiss, M.; Spahn, F.] Univ Potsdam, AG Nichtlineare Dynam, D-14469 Potsdam, Germany. [Strobel, D. F.] Johns Hopkins Univ, Dept Earth & Planetary Sci, Baltimore, MD 21218 USA. [McAndrews, H. J.; Tokar, R.; Wilson, R. J.] Los Alamos Natl Lab, Los Alamos, NM 87545 USA. RP Jones, GH (reprint author), Max Planck Inst Sonnensystemforsch, Max Planck Str 2, D-37191 Katlenburg Lindau, Germany. EM ghj@mssl.ucl.ac.uk RI Roussos, Elias/H-2249-2011; Coates, Andrew/C-2396-2008; Wilson, Rob/C-2689-2009; Jones, Geraint/C-1682-2008; Paranicas, Christopher/B-1470-2016; OI Jones, Geraint/0000-0002-5859-1136; Coates, Andrew/0000-0002-6185-3125; Wilson, Rob/0000-0001-9276-2368; Paranicas, Christopher/0000-0002-4391-8255; Dandouras, Iannis/0000-0002-7121-1118; KEMPF, SASCHA/0000-0001-5236-3004; Hospodarsky, George/0000-0001-9200-9878; Roussos, Elias/0000-0002-5699-0678; Kurth, William/0000-0002-5471-6202 FU Science and Technology Facilities Council [PP/D00084X/1] NR 22 TC 41 Z9 41 U1 1 U2 4 PU AMER ASSOC ADVANCEMENT SCIENCE PI WASHINGTON PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 USA SN 0036-8075 J9 SCIENCE JI Science PD MAR 7 PY 2008 VL 319 IS 5868 BP 1380 EP 1384 DI 10.1126/science.1151524 PG 5 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 270HW UT WOS:000253712900041 PM 18323452 ER PT J AU Connor, BJ Boesch, H Toon, G Sen, B Miller, C Crisp, D AF Connor, Brian J. Boesch, Hartmut Toon, Geoffrey Sen, Bhaswar Miller, Charles Crisp, David TI Orbiting carbon observatory: Inverse method and prospective error analysis SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID ATMOSPHERIC CO2; WFM-DOAS; CM(-1); (CO2)-C-12-O-16 AB The objective, design, and implementation of the OCO inverse method are presented. The inverse method is the algorithm which finds the profile-weighted mean mixing ratio, X-CO2, which best fits the measured spectrum, given a "forward model'' which calculates the spectrum for a given atmospheric state, surface, and instrument properties. Minimizing bias among comparative values of X-CO2 is a critical objective. The algorithm uses an "optimal,'' maximum a posteriori inverse method, with weak a priori constraint, and employs a state vector containing atmospheric and surface properties expected to vary significantly between soundings. An extensive operational characterization and error analysis will be employed, producing quantities designed to aid atmospheric modelers in use of the OCO data. In particular, comparison to inverse models of surface CO2 flux will require use of the OCO column averaging kernel and a priori state vector. An off-line error analysis has also been developed for more detailed error studies, and its use is illustrated by prospective application to case studies of nadir observations in summer and winter at three sites. Uncertainties due to noise, geophysical variability, and spectroscopic parameters are considered in detail. At low and midlatitudes, the single-sounding errors due to these sources are expected to be similar to 0.7-0.8 ppm for high-sun conditions and similar to 1.5-2.5 ppm for low sun (winter). Errors from the same sources in semimonthly regional averages are predicted to be < 1 ppm for all conditions. C1 [Connor, Brian J.] Natl Inst Water & Atmospher Res, Lauder, New Zealand. [Boesch, Hartmut; Toon, Geoffrey; Sen, Bhaswar; Miller, Charles; Crisp, David] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Connor, BJ (reprint author), Natl Inst Water & Atmospher Res, Pvt Bag 50061, Lauder, New Zealand. EM b.connor@niwa.co.nz RI Boesch, Hartmut/G-6021-2012 NR 18 TC 89 Z9 90 U1 5 U2 18 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 MAR 6 PY 2008 VL 113 IS D5 AR D05305 DI 10.1029/2006JD008336 PG 14 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 276QI UT WOS:000254156800001 ER PT J AU Sayres, DS Smith, JB Pittman, JV Weinstock, EM Anderson, JG Heymsfield, G Li, L Fridlind, AM Ackerman, AS AF Sayres, D. S. Smith, J. B. Pittman, J. V. Weinstock, E. M. Anderson, J. G. Heymsfield, G. Li, L. Fridlind, A. M. Ackerman, A. S. TI Validation and determination of ice water content-radar reflectivity relationships during CRYSTAL-FACE: Flight requirements for future comparisons SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID IN-SITU DATA; RADIATIVE PROPERTIES; CIRRUS CLOUDS; PART II; LIDAR; SIZE; VARIABILITY; RETRIEVALS; AIRCRAFT; MISSION AB In situ measurements of cirrus ice water content (IWC) by the Harvard water vapor and total water instruments during Cirrus Regional Study of Tropical Anvils and Cirrus Layers-Florida Area Cirrus Experiment are compared with remote sensing data made by the Cloud Radar System instrument in order to derive and validate an empirical IWC-radar relflectivity Z(e) relationship. The comparisons show that for measurements of in situ IWC and remotely measured radar reflectivity, collocated within 2 km of each other, a single IWC-Z(e) relationship can be found that fits the data with an uncertainty of +/- 20-30%. A cloud resolving model shows this level of uncertainty to be consistent with sampling errors associated with comparing two measurements that are not collocated. Uncertainties are quantified in the use of in situ data to validate the retrieval algorithms used to derive the IWC of clouds from remote sensing observations, such as radar reflectivity Ze. Uncertainties are classified into instrumental uncertainties, uncertainties related to sampling errors, and uncertainties in using a single IWC-Z(e) relationship to describe a cloud. C1 [Sayres, D. S.; Smith, J. B.; Pittman, J. V.; Weinstock, E. M.; Anderson, J. G.] Harvard Univ, Sch Med, Dept Earth & Planetary Sci, Cambridge, MA 02138 USA. [Fridlind, A. M.; Ackerman, A. S.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA. [Heymsfield, G.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Li, L.] Univ Maryland, Baltimore, MD 21250 USA. [Pittman, J. V.] NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA. RP Sayres, DS (reprint author), Harvard Univ, Sch Med, Dept Earth & Planetary Sci, 20 Oxford St, Cambridge, MA 02138 USA. EM sayres@huarp.harvard.edu RI Ackerman, Andrew/D-4433-2012; Fridlind, Ann/E-1495-2012 OI Ackerman, Andrew/0000-0003-0254-6253; NR 28 TC 6 Z9 6 U1 1 U2 4 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 MAR 6 PY 2008 VL 113 IS D5 AR D05208 DI 10.1029/2007JD008847 PG 10 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 276QI UT WOS:000254156800003 ER PT J AU Hwang, SJ Bowman, RC Reiter, JW Rijssenbeek, J Soloveichik, GL Zhao, JC Kabbour, H Ahn, CC AF Hwang, Son-Jong Bowman, Robert C., Jr. Reiter, Joseph W. Rijssenbeek, Job Soloveichik, Grigorii L. Zhao, Ji-Cheng Kabbour, Houria Ahn, Channing C. TI NMR confirmation for formation of [B12H12](2-) complexes during hydrogen desorption from metal borohydrides SO JOURNAL OF PHYSICAL CHEMISTRY C LA English DT Letter ID SOLID-STATE NMR; MAGNESIUM BOROHYDRIDE; CROSS-POLARIZATION; STORAGE MATERIALS; B12H12-2 ION; LIBH4; DECOMPOSITION; COMPOSITES; MG(BH4)(2); ADDITIVES AB B-11 NMR spectroscopy has been employed to identify the reaction intermediates and products formed in the amorphous phase during the thermal hydrogen desorption of metal tetrahydroborates (borohydrides) LiBH4, Mg(BH4)(2), LiSc(BH4)(4), and the mixed Ca(AIH(4))(2)-LiBH4 system. The B-11 magic angle spinning (MAS) and cross polarization magic angle spinning (CPMAS) spectral features of the amorphous intermediate species closely coincide with those of a model compound, closo-borane K2B12H12 that contains the [B12H12](2-) anion. The presence of [B12H12](2-) in the partially decomposed borohydrides was further confirmed by high-resolution solution B-11 and H-1 NMR spectra after dissolution of the intermediate desorption powders in water. The formation of the closo-borane structure is observed as a major intermediate species in all of the metal borohydride systems we have examined. C1 [Hwang, Son-Jong] CALTECH, Div Chem & Chem Engn, Pasadena, CA 91125 USA. [Bowman, Robert C., Jr.; Reiter, Joseph W.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Rijssenbeek, Job; Soloveichik, Grigorii L.; Zhao, Ji-Cheng] GE Global Res, New York, NY 12309 USA. [Kabbour, Houria; Ahn, Channing C.] CALTECH, Div Engn & Appl Sci, Pasadena, CA 91125 USA. RP Hwang, SJ (reprint author), CALTECH, Div Chem & Chem Engn, Pasadena, CA 91125 USA. RI Zhao, Ji-Cheng (JC)/H-4387-2012 OI Zhao, Ji-Cheng (JC)/0000-0002-4426-1080 NR 50 TC 207 Z9 209 U1 7 U2 60 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 MAR 6 PY 2008 VL 112 IS 9 BP 3164 EP 3169 DI 10.1021/jp710894t PG 6 WC Chemistry, Physical; Nanoscience & Nanotechnology; Materials Science, Multidisciplinary SC Chemistry; Science & Technology - Other Topics; Materials Science GA 267MF UT WOS:000253512400002 ER PT J AU Kobayashi, DR Polovina, JJ Parker, DM Kamezaki, N Cheng, IJ Uchida, I Dutton, PH Balazs, GH AF Kobayashi, Donald R. Polovina, Jeffrey J. Parker, Denise M. Kamezaki, Naoki Cheng, I-Jiunn Uchida, Itaru Dutton, Peter H. Balazs, George H. TI Pelagic habitat characterization of loggerhead sea turtles, Caretta caretta, in the North Pacific Ocean (1997-2006): Insights from satellite tag tracking and remotely sensed data SO JOURNAL OF EXPERIMENTAL MARINE BIOLOGY AND ECOLOGY LA English DT Article DE biotelemetry; habitat use; oceanography; remote sensing; resource utilization; satellite tracking; sea turtles ID DIEL VERTICAL MIGRATION; FLIPPER BEAT FREQUENCY; MARINE PROTECTED AREAS; TIGER SHARKS; SELECTIVE PREDATION; SEAGRASS ECOSYSTEM; ELECTIVITY INDEXES; FORAGING BEHAVIOR; DIVING BEHAVIOR; ANIMAL BEHAVIOR AB We analyzed satellite track data for 186 loggerhead sea turtles in the North Pacific Ocean using remotely sensed environmental data to characterize pelagic habitat. A large number of candidate habitat variables were merged to the satellite track data and statistically compared to background values over a large spatiotemporal grid which bounded overall occupancy. Five statistically significant variables were identified out of the 16 environmental variables examined. Two of these variables have strong seasonal, interannual, and spatial patterns (sea surface temperature and chlorophyll a concentration), while three others were primarily spatial (earth magnetic force, earth magnetic declination, and earth magnetic inclination). Habitat selectivity for these variables was quantified using preference curve methodology established in the foraging literature. The output from the selectivity curves was used to predict a multivariate loggerhead sea turtle habitat index across the pelagic North Pacific. This predicted habitat was ground-truthed with newly available satellite track data. (C) 2008 Elsevier B.V. All rights reserved. C1 [Kobayashi, Donald R.; Polovina, Jeffrey J.; Parker, Denise M.; Balazs, George H.] NOAA, Pacific Isl Fisheries Sci Ctr, Natl Marine Fisheries Serv, US Dept Commerce, Honolulu, HI 96822 USA. [Kobayashi, Donald R.] Univ Technol Sydney, Dept Environm Sci, Broadway, NSW 2007, Australia. [Parker, Denise M.] Univ Hawaii, Joint Inst Marine & Atmospher Res, Honolulu, HI 96822 USA. [Kamezaki, Naoki] Sea Turtle Assoc Japan, Osaka 5730163, Japan. [Cheng, I-Jiunn] Natl Taiwan Ocean Univ, Inst Marine Biol, Chilung 20224, Taiwan. [Uchida, Itaru] Port Nagoya Publ Aquarium, Minato Ku, Nagoya, Aichi 4550033, Japan. [Dutton, Peter H.] NOAA, SW Fisheries Sci Ctr, Natl Marine Fisheries Serv, US Dept Commerce, La Jolla, CA 92037 USA. RP Kobayashi, DR (reprint author), NOAA, Pacific Isl Fisheries Sci Ctr, Natl Marine Fisheries Serv, US Dept Commerce, 2570 Dole St, Honolulu, HI 96822 USA. EM Donald.Kobayashi@noaa.gov NR 91 TC 54 Z9 60 U1 4 U2 52 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0022-0981 EI 1879-1697 J9 J EXP MAR BIOL ECOL JI J. Exp. Mar. Biol. Ecol. PD MAR 3 PY 2008 VL 356 IS 1-2 BP 96 EP 114 DI 10.1016/j.jembe.2007.12.019 PG 19 WC Ecology; Marine & Freshwater Biology SC Environmental Sciences & Ecology; Marine & Freshwater Biology GA 284CN UT WOS:000254683000008 ER PT J AU Rice, MR Balazs, GH AF Rice, Marc R. Balazs, George H. TI Diving behavior of the Hawaiian green turtle (Chelonia mydas) during oceanic migrations SO JOURNAL OF EXPERIMENTAL MARINE BIOLOGY AND ECOLOGY LA English DT Article DE diving; Hawaiian islands; migration; sea turtles; TDR ID SEA-TURTLES; ASCENSION ISLAND; DIVE PROFILES; LEPIDOCHELYS-OLIVACEA; SATELLITE TRACKING; DEPTH DISTRIBUTION; DURATIONS; PACIFIC AB The diving behavior of an adult female and two adult male green turtles was recorded during their roundtrip breeding migration from Laniakea, Oahu, to French Frigate Shoals in the Northwestern Hawaiian Islands. These data represent the first detailed records of diving behavior of green turtles as they migrate to their breeding grounds. All three turtles exhibited a biphasic diving behavior. During the daylight hours, diving depth was shallow (1-4 m) and duration was short (1-18 min). It was assumed that the turtles were moving deliberately toward their destination during this time. Between 1900 and 1930 h daily, the turtles began a diving pattern consisting of deep dives with a mean maximum dive depth of 35-55 m and a mean duration of 35 to 44 min. The shallow diurnal diving began between 0600 and 0700 h, after the nocturnal deep-diving pattern ended. The adult female made two dives in excess of 135 to and one male made several dives in excess of 100 in. These are the deepest dives ever recorded for a naturally diving green turtle. It took an average of 36 days for the turtles to make the trip to French Frigate Shoals and an average of 30 days to make the return trip. The deep nocturnal diving was unexpected and this behavior is in need of further investigation. (C) 2008 Elsevier B.V All rights reserved. C1 [Rice, Marc R.] Hawaii Preparatory Acad, Kamuela, HI 96743 USA. [Balazs, George H.] NOAA, Natl Marine Fisheries Serv, Pacific Isl Fisheries Sci Ctr, Honolulu, HI 96822 USA. RP Rice, MR (reprint author), Hawaii Preparatory Acad, 65-1692 Kohala Mt Rd, Kamuela, HI 96743 USA. EM mrice@hpa.edu NR 33 TC 25 Z9 27 U1 3 U2 10 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0022-0981 EI 1879-1697 J9 J EXP MAR BIOL ECOL JI J. Exp. Mar. Biol. Ecol. PD MAR 3 PY 2008 VL 356 IS 1-2 BP 121 EP 127 DI 10.1016/j.jembe.2007.12.010 PG 7 WC Ecology; Marine & Freshwater Biology SC Environmental Sciences & Ecology; Marine & Freshwater Biology GA 284CN UT WOS:000254683000010 ER PT J AU Suh, JO Tu, KN Lutsenko, GV Gusak, AM AF Suh, J. O. Tu, K. N. Lutsenko, G. V. Gusak, A. M. TI Size distribution and morphology of Cu(6)Sn(5) scallops in wetting reaction between molten solder and copper SO ACTA MATERIALIA LA English DT Article DE CU(6)Sn(5); solder wetting; ripening ID KINETICS; ALLOY; CU AB During the reaction between molten solder and copper, ripening and growth Of Cu(6)Sn(5) scallops take place at the solder/metal interface. An experimental study on the morphology, size distribution and growth rate Of Cu(6)Sn(5) scallops was conducted. The measured size distributions Of CU(6)Sn(5) as a function of time from top-view and cross-sectional view scanning electron microscopy images were in good agreement with the flux-driven ripening (FDR) theory. The FDR theory assumes a non-conservative ripening under a constant total interfacial area between the scallops and the solder, while the total volume of scallops increases with reaction time. The measured average radius of the scallops was proportional to the cube root of time. Comparing the experimental results and the theoretical model, the width of the liquid channel between scallops was calculated to be similar to 2.5 nm. Morphology of the scallop-type CU(6)Sn(5) was dependent to the composition of the solder. The scallop morphology became more faceted when the composition was further away from the eutectic composition. The CU(6)Sn(5) scallops with a shape close to hemispheric gave better agreement with FDR theory. The small difference between the experimental data and theory was explained by taking the noise factor into account. The modified FDR model showed even better agreement with the experimental data. (c) 2007 Acta Materialia Inc. Published by Elsevier Ltd. All rights reserved. C1 [Suh, J. O.; Tu, K. N.] Univ Calif Los Angeles, Dept Mat Sci & Engn, Los Angeles, CA 90095 USA. [Lutsenko, G. V.; Gusak, A. M.] Cherkasy Natl Univ, Dept Theoret Phys, Cherkassy, Ukraine. RP Suh, JO (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. EM Jong-ook.Suh@jpl.nasa.gov RI Gusak, Andriy/F-3459-2010; Lutsenko, Galyna/C-2321-2014 OI Gusak, Andriy/0000-0002-2594-5559; Lutsenko, Galyna/0000-0002-9727-7836 NR 13 TC 64 Z9 66 U1 3 U2 23 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 1359-6454 J9 ACTA MATER JI Acta Mater. PD MAR PY 2008 VL 56 IS 5 BP 1075 EP 1083 DI 10.1016/j.actamat.2007.11.009 PG 9 WC Materials Science, Multidisciplinary; Metallurgy & Metallurgical Engineering SC Materials Science; Metallurgy & Metallurgical Engineering GA 276ZU UT WOS:000254183000017 ER PT J AU Davis, RB Virgin, LN Brown, AM AF Davis, R. Benjamin Virgin, Lawrence N. Brown, Andrew M. TI Cylindrical shell submerged in bounded acoustic media: A modal approach SO AIAA JOURNAL LA English DT Article; Proceedings Paper CT AIAA/ASME/ASCE/AHS/ASC 48th Structures, Structural Dynamics, and Materials Conference CY APR 23-26, 2007 CL Honolulu, HI SP AIAA, ASME, ASCE, AHS, ASC ID SYSTEMS; FLUID; NOISE AB The dynamics of a simply supported cylindrical shell submerged in liquid hydrogen and liquid oxygen are considered. The shell itself is bounded by a rigid outer cylinder with closed rigid ends. This configuration gives rise to two fluid-filled cavities-an inner cylindrical cavity. and an outer annular cavity. Such geometries are common in rocket engine design. The natural frequencies and modes of the fluid-structure system are computed by combining the rigid wall acoustic cavity modes and the in vacuo structural modes into a system of coupled ordinary differential equations. Eigenvalue veering is observed near the intersections of the curves representing natural frequencies of the rigid wall acoustic and the in vacuo structural modes. In the case of a shell submerged in liquid hydrogen, system frequencies near these intersections are as much as 30% lower than the corresponding in vacuo structural frequencies. Because of its high density, the frequency reductions in the presence of liquid oxygen are even more dramatic. The forced responses of a shell submerged in liquid hydrogen and liquid oxygen, while subject to a harmonic point excitation, are also presented. The responses in the presence of fluid are found to be quite distinct from those of the structure in vacuo. C1 [Davis, R. Benjamin] Duke Univ, Dept Mech Engn & Mat Sci, Durham, NC 27708 USA. [Virgin, Lawrence N.] Duke Univ, Dept Civil & Environm Engn, Durham, NC 27708 USA. [Brown, Andrew M.] NASA, George C Marshall Space Flight Ctr, Struct & Dynam Analysis Branch, Huntsville, AL 35812 USA. RP Davis, RB (reprint author), Duke Univ, Dept Mech Engn & Mat Sci, Durham, NC 27708 USA. OI Davis, R Benjamin /0000-0003-4478-302X NR 19 TC 2 Z9 2 U1 0 U2 3 PU AMER INST AERONAUT ASTRONAUT PI RESTON PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA SN 0001-1452 J9 AIAA J JI AIAA J. PD MAR PY 2008 VL 46 IS 3 BP 752 EP 763 DI 10.2514/1.31706 PG 12 WC Engineering, Aerospace SC Engineering GA 266AL UT WOS:000253403200020 ER PT J AU Koch, GJ Beyon, JY Gibert, F Barnes, BW Ismail, S Petros, M Petzar, PJ Yu, J Modlin, EA Davis, KJ Singh, UN AF Koch, Grady J. Beyon, Jeffrey Y. Gibert, Fabien Barnes, Bruce W. Ismail, Syed Petros, Mulugeta Petzar, Paul J. Yu, Jirong Modlin, Edward A. Davis, Kenneth J. Singh, Upendra N. TI Side-line tunable laser transmitter for differential absorption lidar measurements of CO2: design and application to atmospheric measurements SO APPLIED OPTICS LA English DT Article ID TALL TOWER; PACIFIC; FOREST AB A 2 mu m wavelength, 90 mJ, 5 Hz pulsed Ho laser is described with wavelength control to precisely tune and lock the wavelength at a desired offset up to 2.9 GHz from the center of a CO2 absorption line. Once detuned from the line center the laser wavelength is actively locked to keep the wavelength within 1.9 MHz standard deviation about the setpoint. This wavelength control allows optimization of the optical depth for a differential absorption lidar (DIAL) measuring atmospheric CO2 concentrations. The laser transmitter has been coupled with a coherent heterodyne receiver for measurements of CO2 concentration using aerosol backscatter; wind and aerosols are also measured with the same lidar and provide useful additional information on atmospheric structure. Range-resolved CO2 measurements were made with < 2.4% standard deviation using 500 m range bins and 6.7 min (1000 pulse pairs) integration time. Measurement of a horizontal column showed a precision of the CO2 concentration to < 0.7% standard deviation using a 30 min (4500 pulse pairs) integration time, and comparison with a collocated in situ sensor showed the DIAL to measure the same trend of a diurnal variation and to detect shorter time scale CO2 perturbations. For vertical column measurements the lidar was setup at the WLEF tall tower site in Wisconsin to provide meteorological profiles and to compare the DIAL measurements with the in situ sensors distributed on the tower up to 396 m height. Assuming the DIAL column measurement extending from 153 m altitude to 1353 m altitude should agree with the tower in situ sensor at 396 m altitude, there was a 7.9 ppm rms difference between the DIAL and the in situ sensor using a 30 min rolling average on the DIAL measurement. (C) 2008 Optical Society of America. C1 [Koch, Grady J.; Barnes, Bruce W.; Ismail, Syed; Yu, Jirong; Modlin, Edward A.; Singh, Upendra N.] NASA, Langley Res Ctr, Hampton, VA 23692 USA. [Beyon, Jeffrey Y.] Calif State Univ Los Angeles, Dept Elect & Comp Engn, Los Angeles, CA 90032 USA. [Gibert, Fabien; Davis, Kenneth J.] Penn State Univ, Dept Meteorol, University Pk, PA 16802 USA. [Petros, Mulugeta] Sci & Technol Corp, Hampton, VA 23666 USA. [Petzar, Paul J.] Natl Inst Aerosp, Hampton, VA 23666 USA. RP Koch, GJ (reprint author), NASA, Langley Res Ctr, Hampton, VA 23692 USA. EM grady.j.koch@nasa.gov NR 24 TC 72 Z9 76 U1 2 U2 18 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 MAR 1 PY 2008 VL 47 IS 7 BP 944 EP 956 DI 10.1364/AO.47.000944 PG 13 WC Optics SC Optics GA 283ZC UT WOS:000254674000011 PM 18311266 ER PT J AU Muterspaugh, MW Lane, BF Fekel, FC Konacki, M Burke, BF Kulkarni, SR Colavita, MM Shao, M Wiktorowicz, SJ AF Muterspaugh, Matthew W. Lane, Benjamin F. Fekel, Francis C. Konacki, Maciej Burke, Bernard F. Kulkarni, S. R. Colavita, M. M. Shao, M. Wiktorowicz, Sloane J. TI Masses, luminosities, and orbital coplanarities of the mu orionis quadruple-star system from phases differential astrometry SO ASTRONOMICAL JOURNAL LA English DT Article DE astrometry; binaries : close; binaries : visual; stars : distances; stars : individual (delta Equ, kappa Peg, mu Orionis, V819 Her); techniques : interferometric ID PALOMAR TESTBED INTERFEROMETER; TRIPLE STARS; SPECKLE OBSERVATIONS; RADIAL-VELOCITIES; BINARY; INCLINATION; ORIENTATION; TELESCOPE; HIPPARCOS; STABILITY AB mu Orionis was identified by spectroscopic studies as a quadruple-star system. Seventeen high-precision differential astrometry measurements of mu Ori have been collected by the Palomar High-precision Astrometric Search for Exoplanet Systems (PHASES). These show both the motion of the long-period binary orbit and short-period perturbations superimposed on that caused by each of the components in the long-period system being themselves binaries. The new measurements enable the orientations of the long-period binary and short-period subsystems to be determined. Recent theoretical work predicts the distribution of relative inclinations between inner and outer orbits of hierarchical systems to peak near 40 and 140 degrees. The degree of coplanarity of this complex system is determined, and the angle between the planes of the A-B and Aa-Ab orbits is found to be 136.7 +/- 8.3 degrees, near the predicted distribution peak at 140 degrees; this result is discussed in the context of the handful of systems with established mutual inclinations. The system distance and masses for each component are obtained from a combined fit of the PHASES astrometry and archival radial velocity observations. The component masses have relative precisions of 5% (component Aa), 15% (Ab), and 1.4% (each of Ba and Bb). The median size of the minor axes of the uncertainty ellipses for the new measurements is 20 micro-arcseconds (mu as). Updated orbits for delta Equulei, kappa Pegasi, and V819 Herculis are also presented. C1 [Muterspaugh, Matthew W.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Lane, Benjamin F.] Charles Stark Draper Lab Inc, Cambridge, MA 02139 USA. [Fekel, Francis C.] Tennessee State Univ, Ctr Excellence Informat Syst, Nashville, TN 37203 USA. [Konacki, Maciej] Polish Acad Sci, Nicholas Copernicus Astronom Ctr, PL-87100 Torun, Poland. [Burke, Bernard F.] MIT, Dept Phys, MIT Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. [Kulkarni, S. R.] CALTECH, Div Phys Math & Astron, Pasadena, CA 91125 USA. [Colavita, M. M.; Shao, M.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Wiktorowicz, Sloane J.] CALTECH, Dept Geol & Planetary Sci, Pasadena, CA 91125 USA. RP Muterspaugh, MW (reprint author), Univ Calif Berkeley, Space Sci Lab, 7 Gauss Way, Berkeley, CA 94720 USA. EM matthew1@ssl.berkeley.edu; blane@mit.edu; maciej@ncac.torun.pl NR 34 TC 35 Z9 35 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 J9 ASTRON J JI Astron. J. PD MAR PY 2008 VL 135 IS 3 BP 766 EP 776 DI 10.1088/0004-6256/135/3/766 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 271WF UT WOS:000253818700002 ER PT J AU Sahai, R Morris, M Contreras, CS Claussen, M AF Sahai, Raghvendra Morris, Mark Sanchez Contreras, Carmen Claussen, Mark TI Preplanetary nebulae: A Hubble space telescope imaging survey and a new morphological classification system (vol 134, pg 2200, 2007) SO ASTRONOMICAL JOURNAL LA English DT Correction C1 [Sahai, Raghvendra] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Morris, Mark] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA. [Sanchez Contreras, Carmen] CSIC, Inst Estructura Mat, Dept Astrofis Mol & Infraroja, E-28006 Madrid, Spain. [Claussen, Mark] Natl Radio Astron Observ, Socorro, NM 87801 USA. RP Sahai, R (reprint author), CALTECH, Jet Prop Lab, MS 183-900, Pasadena, CA 91109 USA. RI Sanchez-Contreras, Carmen/N-3718-2015 OI Sanchez-Contreras, Carmen/0000-0002-6341-592X NR 1 TC 0 Z9 0 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 J9 ASTRON J JI Astron. J. PD MAR PY 2008 VL 135 IS 3 BP 1099 EP 1099 DI 10.1088/0004-6256/135/3/1099 PG 1 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 271WF UT WOS:000253818700031 ER PT J AU Mahabal, A Djorgovski, SG Turmon, M Jewell, J Williams, RR Drake, AJ Graham, MG Donalek, C Glikman, E AF Mahabal, A. Djorgovski, S. G. Turmon, M. Jewell, J. Williams, R. R. Drake, A. J. Graham, M. G. Donalek, C. Glikman, E. CA Palomar-Quest Team TI Automated probabilistic classification of transients and variables SO ASTRONOMISCHE NACHRICHTEN LA English DT Article; Proceedings Paper CT Workshop on Hot-Wiring the Transient Universe CY JUN 04-07, 2007 CL Tucson, AZ SP VOEvent Working Grp, Heterogeneous Telescope Networks DE astronomical databases : miscellaneous; methods : data analysis; methods : statistical; surveys AB There is an increasing number of large, digital, synoptic sky surveys, in which repeated observations are obtained over large areas of the sky in multiple epochs. Likewise, there is a growth in the number of (often automated or robotic) follow-up facilities with varied capabilities in terms of instruments, depth, cadence, wavelengths, etc., most of which are geared toward some specific astrophysical phenomenon. As the number of detected transient events grows, an automated, probabilistic classification of the detected variables and transients becomes increasingly important, so that an optimal use can be made of follow-up facilities, without unnecessary duplication of effort. We describe a methodology now under development for a prototype event classification system; it involves Bayesian and Machine Learning classifiers, automated incorporation of feedback from follow-up observations, and discriminated or directed follow-up requests. This type of methodology may be essential for the massive synoptic sky surveys in the future. (C) 2008 WILEY-VCH Verlag GmbH & Co. KGaA, Weinheim. C1 [Mahabal, A.; Djorgovski, S. G.; Williams, R. R.; Drake, A. J.; Graham, M. G.; Donalek, C.; Glikman, E.] CALTECH, Pasadena, CA 91125 USA. [Turmon, M.; Jewell, J.] Jet Propuls Lab, Pasadena, CA USA. RP Mahabal, A (reprint author), CALTECH, Pasadena, CA 91125 USA. EM aam@astro.caltech.edu NR 14 TC 28 Z9 28 U1 0 U2 2 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 MAR PY 2008 VL 329 IS 3 BP 288 EP 291 DI 10.1002/asna.200710943 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 282CW UT WOS:000254546200018 ER PT J AU Barthelmy, S AF Barthelmy, S. TI GCN and VOEvent: A status report SO ASTRONOMISCHE NACHRICHTEN LA English DT Article; Proceedings Paper CT Workshop on Hot-Wiring the Transient Universe CY JUN 04-07, 2007 CL Tucson, AZ SP VOEvent Working Grp, Heterogeneous Telescope Networks DE astronomical databases : miscellaneous; gamma-rays : bursts AB The GRB Coordinates Network (GCN) has filled an important niche in the conduct and progress of research on GRB for more than 14 years. The methods used to collect and distribute the positions, lightcurves, spectra, and images on GRB in real time (a few seconds) will be reviewed. For the research on GRBs to continue to move forward and for other fields of transient astronomy to move forward, enhancements are needed to the GCN. VOEvents is one of those changes, and that addition will be described here. The enhanced system will be called VO-GCN. (c) 2008 WILEY-VCH Verlag GmbH&Co. KGaA. Weinheim. C1 NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Barthelmy, S (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. EM scott@milkyway.gsfc.nasa.gov RI Barthelmy, Scott/D-2943-2012 NR 2 TC 6 Z9 6 U1 0 U2 2 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 MAR PY 2008 VL 329 IS 3 BP 340 EP 342 DI 10.1002/asna.200710954 PG 3 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 282CW UT WOS:000254546200033 ER PT J AU van der Horst, AJ Kamble, A Resmi, L Wijers, RAMJ Bhattacharya, D Scheers, B Rol, E Strom, R Kouveliotou, C Oosterloo, T Ishwara-Chandra, CH AF van der Horst, A. J. Kamble, A. Resmi, L. Wijers, R. A. M. J. Bhattacharya, D. Scheers, B. Rol, E. Strom, R. Kouveliotou, C. Oosterloo, T. Ishwara-Chandra, C. H. TI Detailed study of the GRB 030329 radio afterglow deep into the non-relativistic phase SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE gamma rays : bursts; radio continuum : general; radiation mechanisms : non-thermal ID GAMMA-RAY BURST; LIGHT-CURVE; JET; CALORIMETRY; SUPERNOVA; MILLIMETER; DYNAMICS; SIZE AB Context. We explore the physics behind one of the brightest radio afterglows ever, GRB 030329, at late times when the jet is non-relativistic. Aims. We determine the physical parameters of the blast wave and its surroundings, in particular the index of the electron energy distribution, the energy of the blast wave, and the density (structure) of the circumburst medium. We then compare our results with those from image size measurements. Methods. We observed the GRB 030329 radio afterglow with the Westerbork Synthesis Radio Telescope and the Giant Metrewave Radio Telescope at frequencies from 325 MHz to 8.4 GHz, spanning a time range of 268-1128 days after the burst. We modeled all the available radio data and derived the physical parameters. Results. The index of the electron energy distribution is p = 2.1, the circumburst medium is homogeneous, and the transition to the non-relativistic phase happens at t(NR) similar to 80 days. The energy of the blast wave and density of the surrounding medium are comparable to previous findings. Conclusions. Our findings indicate that the blast wave is roughly spherical at t(NR), and they agree with the implications from the VLBI studies of image size evolution. It is not clear from the presented dataset whether we have seen emission from the counter jet or not. We predict that the Low Frequency Array will be able to observe the afterglow of GRB 030329 and many other radio afterglows, constraining the physics of the blast wave during its non-relativistic phase even further. C1 [van der Horst, A. J.; Wijers, R. A. M. J.; Scheers, B.; Strom, R.] Univ Amsterdam, Astron Inst, NL-1098 SJ Amsterdam, Netherlands. [Kamble, A.; Resmi, L.; Bhattacharya, D.] Raman Res Inst, Bangalore 560080, Karnataka, India. [Resmi, L.] Indian Inst Sci, Joint Astron Programme, Bangalore 560012, Karnataka, India. [Bhattacharya, D.] Inter Univ Ctr Astron & Astrophys, Pune 411007, Maharashtra, India. [Rol, E.] Univ Leicester, Dept Phys & Astron, Leicester LE2 7RH, Leics, England. [Strom, R.; Oosterloo, T.] ASTRON, NL-7990 AA Dwingeloo, Netherlands. [Kouveliotou, C.] NSSTC, MSFC, NASA, Huntsville, AL USA. [Ishwara-Chandra, C. H.] Natl Ctr Radio Astrophys, Pune 411007, Maharashtra, India. RP van der Horst, AJ (reprint author), Univ Amsterdam, Astron Inst, Kruislaan 403, NL-1098 SJ Amsterdam, Netherlands. EM avdhorst@science.uva.nl RI M, Manjunath/N-4000-2014; Bhattacharya, Dipankar/J-6927-2015; OI M, Manjunath/0000-0001-8710-0730; Bhattacharya, Dipankar/0000-0003-3352-3142; Wijers, Ralph/0000-0002-3101-1808 NR 31 TC 36 Z9 36 U1 0 U2 3 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD MAR PY 2008 VL 480 IS 1 BP 35 EP 43 DI 10.1051/0004-6361:20078051 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 268JP UT WOS:000253576400009 ER PT J AU Raiteri, CM Villata, M Larionov, VM Aller, MF Bach, U Gurwell, M Kurtanidze, OM Lahteenmaki, A Nilsson, K Volvach, A Aller, HD Arkharov, AA Bachev, R Berdyugin, A Bottcher, M Buemi, CS Calcidese, P Cozzi, E Di Paola, A Dolci, M Fan, JH Forne, E Foschini, L Gupta, AC Hagen-Thorn, VA Hooks, L Hovatta, T Joshi, M Kadler, M Kimeridze, GN Konstantinova, TS Kostov, A Krichbaum, TP Lanteri, L Larionova, LV Lee, CU Leto, P Lindfors, E Montagni, F Nesci, R Nieppola, E Nikolashvili, MG Ohlert, J Oksanen, A Ovcharov, E Paakkonen, P Pasanen, M Pursimo, T Ros, JA Semkov, E Sigua, LA Smart, RL Strigachev, A Takalo, LO Torii, K Torniainen, I Tornikoski, M Trigilio, C Tsunemi, H Umana, G Valcheva, A AF Raiteri, C. M. Villata, M. Larionov, V. M. Aller, M. F. Bach, U. Gurwell, M. Kurtanidze, O. M. Lahteenmaki, A. Nilsson, K. Volvach, A. Aller, H. D. Arkharov, A. A. Bachev, R. Berdyugin, A. Boettcher, M. Buemi, C. S. Calcidese, P. Cozzi, E. Di Paola, A. Dolci, M. Fan, J. H. Forne, E. Foschini, L. Gupta, A. C. Hagen-Thorn, V. A. Hooks, L. Hovatta, T. Joshi, M. Kadler, M. Kimeridze, G. N. Konstantinova, T. S. Kostov, A. Krichbaum, T. P. Lanteri, L. Larionova, L. V. Lee, C. -U. Leto, P. Lindfors, E. Montagni, F. Nesci, R. Nieppola, E. Nikolashvili, M. G. Ohlert, J. Oksanen, A. Ovcharov, E. Paakkonen, P. Pasanen, M. Pursimo, T. Ros, J. A. Semkov, E. Sigua, L. A. Smart, R. L. Strigachev, A. Takalo, L. O. Torii, K. Torniainen, I. Tornikoski, M. Trigilio, C. Tsunemi, H. Umana, G. Valcheva, A. TI Radio-to-UV monitoring of AO 0235+164 by the WEBT and Swift during the 2006-2007 outburst SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE galaxies : active; galaxies : BL Lacertae objects : general; galaxies : BL Lacertae objects : individual : AO 0235+164; galaxies : jets; galaxies : quasars : general ID XMM-NEWTON OBSERVATIONS; BL-LACERTAE; AO 0235+164; LIGHT CURVES; HELICAL JETS; VARIABILITY; CAMPAIGN; BLAZARS; STARS; FIELD AB Context. The blazar AO 0235+164 was claimed to show a quasi-periodic behaviour in the radio and optical bands in the past, with the main outbursts repeating every 5-6 years. However, the predicted 2004 outburst did not occur, and further analysis suggested a longer time scale, according to which the next event would have occurred in the 2006-2007 observing season. Moreover, an extra emission component contributing to the UV and soft X-ray flux was detected, whose nature is not yet clear. An optical outburst was observed in late 2006-early 2007, which triggered a Whole Earth Blazar Telescope (WEBT) campaign as well as target of opportunity (ToO) observations by the Swift satellite. Aims. In this paper, we present the radio-to-optical data taken by the WEBT together with the UV data acquired by the UltraViolet and Optical Telescope (UVOT) instrument onboard Swift to investigate both the outburst behaviour at different wavelengths and the nature of the extra emission component. Methods. Multifrequency light curves have been assembled with data from 27 observatories; optical and UV fluxes have been cleaned from the contamination of the southern active galactic nucleus (AGN). We have analysed spectral energy distributions at different epochs, corresponding to different brightness states; extra absorption by the foreground galaxy has been taken into account. Results. We found the optical outburst to be as strong as the big outbursts of the past: starting from late September 2006, a brightness increase of similar to 5 mag led to the outburst peak in February 19-21, 2007. We also observed an outburst at mm and then at cm wavelengths, with an increasing time delay going toward lower frequencies during the rising phase. Cross-correlation analysis indicates that the 1 mm and 37 GHz flux variations lagged behind the R-band ones by about 3 weeks and 2 months, respectively. These short time delays suggest that the corresponding jet emitting regions are only slightly separated and/or misaligned. In contrast, during the outburst decreasing phase the flux faded contemporaneously at all cm wavelengths. This abrupt change in the emission behaviour may suggest the presence of some "shutdown" mechanism of intrinsic or geometric nature. The behaviour of the UV flux closely follows the optical and near-IR one. By separating the synchrotron and extra component contributions to the UV flux, we found that they correlate, which suggests that the two emissions have a common origin. C1 [Raiteri, C. M.; Villata, M.; Lanteri, L.; Smart, R. L.] Osserv Astron Torino, INAF, Turin, Italy. [Larionov, V. M.; Hagen-Thorn, V. A.; Konstantinova, T. S.; Larionova, L. V.] St Petersburg State Univ, Astron Inst, St Petersburg, Russia. [Aller, M. F.; Aller, H. D.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Larionov, V. M.] Pulkovo Observ, St Petersburg, Russia. [Bach, U.] Max Planck Inst Radioastron, D-5300 Bonn, Germany. [Gurwell, M.] Harvard Smithsonian Ctr Astroph, Cambridge, MA USA. [Lahteenmaki, A.; Hovatta, T.; Nieppola, E.; Torniainen, I.; Tornikoski, M.] Helsinki Univ Technol, Metsahovi Radio Obs, FIN-02150 Espoo, Finland. [Nilsson, K.; Berdyugin, A.; Lindfors, E.; Pasanen, M.; Takalo, L. O.] Univ Turku, Tuorla Observ, Piikkio, Finland. [Bachev, R.; Semkov, E.; Strigachev, A.; Valcheva, A.] Bulgarian Acad Sci, Inst Astron, Sofia, Bulgaria. [Boettcher, M.; Hooks, L.; Joshi, M.] Ohio Univ, Dept Phys & Astron, Athens, OH 45701 USA. [Di Paola, A.] Osserv Astron Roma, INAF, Rome, Italy. [Fan, J. H.] Guangzhou Univ, Ctr Astrophys, Guangzhou 510405, Guangdong, Peoples R China. [Forne, E.] Agrupacio Astron Sabadell, Sabadell, Spain. [Foschini, L.] IASF Bologna, INAF, Bologna, Italy. [Gupta, A. C.] Chinese Acad Sci, YNAO, Kunming, Peoples R China. [Kadler, M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Krichbaum, T. P.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Lee, C. -U.] Korea Astron & Space Sci Inst, Taejon, South Korea. [Nesci, R.] Univ Roma La Sapienza, Dept Phys, Rome, Italy. [Ohlert, J.] Michael Adrian Observ, Trebur, Germany. [Ovcharov, E.; Valcheva, A.] Univ Sofia, Sofia, Bulgaria. [Paakkonen, P.] Univ Joensuu, Jakokoski Observ, FIN-80101 Joensuu, Finland. [Pursimo, T.] Nord Opt Telescope, Santa Cruz de La Palma, Spain. [Torii, K.] Osaka Univ, Suita, Osaka 565, Japan. RP Raiteri, CM (reprint author), Osserv Astron Torino, INAF, Turin, Italy. EM raiteri@oato.inaf.it; villata@oato.inaf.it RI Foschini, Luigi/H-3833-2012; Larionov, Valeri/H-1349-2013; Lahteenmaki, Anne/L-5987-2013; Kurtanidze, Omar/J-6237-2014; Grishina, Tatiana/H-6873-2013; Hagen-Thorn, Vladimir/H-3983-2013; OI Foschini, Luigi/0000-0001-8678-0324; Larionov, Valeri/0000-0002-4640-4356; Grishina, Tatiana/0000-0002-3953-6676; Hagen-Thorn, Vladimir/0000-0002-6431-8590; Larionova, Liudmila/0000-0002-0274-1481; Buemi, Carla Simona/0000-0002-7288-4613; Leto, Paolo/0000-0003-4864-2806; Di Paola, Andrea/0000-0002-2189-8644; Villata, Massimo/0000-0003-1743-6946; Raiteri, Claudia Maria/0000-0003-1784-2784 NR 34 TC 40 Z9 40 U1 0 U2 2 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD MAR PY 2008 VL 480 IS 2 BP 339 EP 347 DI 10.1051/0004-6361:20079044 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 271RP UT WOS:000253806700009 ER PT J AU Masetti, N Mason, E Landi, R Giommi, P Bassani, L Malizia, A Bird, AJ Bazzano, A Dean, AJ Gehrels, N Palazzi, E Ubertini, P AF Masetti, N. Mason, E. Landi, R. Giommi, P. Bassani, L. Malizia, A. Bird, A. J. Bazzano, A. Dean, A. J. Gehrels, N. Palazzi, E. Ubertini, P. TI High-redshift blazar identification for Swift j1656.3-3302 SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE quasars : emission lines; quasars : individual : J1656.3-3302 galaxies : high-redshift; galaxies : active; X-rays : galaxies; astrometry ID RADIO-LOUD QUASARS; SOUTHERN SPECTROPHOTOMETRIC STANDARDS; RAY SURVEY CATALOG; SPECTROSCOPY; TELESCOPE; EMISSION; SPECTRA; MISSION; OBJECTS; IMAGER AB We report on the high-redshift blazar identification of a new gamma-ray source, Swift J1656.3-3302, detected with the BAT imager onboard the Swift satellite and the IBIS instrument on the INTEGRAL satellite. Follow-up optical spectroscopy has allowed us to identify the counterpart as an R similar to 19 mag source that shows broad Lyman-alpha, Si IV, He II, C IV, and CIII] emission lines at redshift z = 2.40 +/- 0.01. Spectral evolution is observed in X-rays when the INTEGRAL/IBIS data are compared to the Swift/BAT results, with the spectrum steepening when the source gets fainter. The 0.7-200 keV X-ray continuum, observed with Swift/XRT and INTEGRAL/ IBIS, shows the power law shape typical of radio loud (broad emission line) active galactic nuclei (with a photon index Gamma similar to 1.6) and a hint of spectral curvature below similar to 2 keV, possibly due to intrinsic absorption (N-H similar to 7 x 10(22) cm(-2)) local to the source. Alternatively, a slope change (Delta Gamma similar to 1) around 2.7 keV can describe the X-ray spectrum equally well. At this redshift, the observed 20-100 keV luminosity of the source is similar to 10(48) erg s(-1) (assuming isotropic emission), making Swift J1656.3-3302 one of the most X-ray luminous blazars. This source is yet another example of a distant gamma-ray loud quasar discovered above 20 keV. It is also the farthest object, among the previously unidentified INTEGRAL sources, whose nature has been determined a posteriori through optical spectroscopy. C1 [Masetti, N.; Landi, R.; Bassani, L.; Malizia, A.; Palazzi, E.] Inst Astrofis Spaziale & Fis Cosm Bologna, INAF, I-40129 Bologna, Italy. [Mason, E.] European So Observ, Santiago 19, Chile. [Giommi, P.] ASI Data Ctr, I-00044 Frascati, Italy. [Dean, A. J.] Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England. [Bazzano, A.] Inst Astrofis Spaziale & Fis Cosm Roma, INAF, I-00133 Rome, Italy. [Gehrels, N.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Masetti, N (reprint author), Inst Astrofis Spaziale & Fis Cosm Bologna, INAF, Via Gobetti 101, I-40129 Bologna, Italy. EM masetti@iasfbo.inaf.it RI Gehrels, Neil/D-2971-2012; Palazzi, Eliana/N-4746-2015; OI mason, elena/0000-0003-3877-0484; giommi, paolo/0000-0002-2265-5003; Malizia, Angela/0000-0002-6558-1163; Palazzi, Eliana/0000-0002-8691-7666; Bassani, Loredana/0000-0003-4858-6963; Masetti, Nicola/0000-0001-9487-7740; Bazzano, Angela/0000-0002-2017-4396 NR 49 TC 14 Z9 14 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 MAR PY 2008 VL 480 IS 3 BP 715 EP 721 DI 10.1051/0004-6361:20078901 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 274IB UT WOS:000253993900015 ER PT J AU Caballero, I Santangelo, A Kretschmar, P Staubert, R Postnov, K Klochkov, D Camero-Arranz, A Finger, MH Kreykenbohm, I Pottschmidt, K Rothschild, RE Suchy, S Wilms, J Wilson, CA AF Caballero, I. Santangelo, A. Kretschmar, P. Staubert, R. Postnov, K. Klochkov, D. Camero-Arranz, A. Finger, M. H. Kreykenbohm, I. Pottschmidt, K. Rothschild, R. E. Suchy, S. Wilms, J. Wilson, C. A. TI The pre-outburst flare of the A 0535+26 August/September 2005 outburst SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE X-rays : binaries; stars : magnetic fields; stars : individual : A 0535+26 ID RAY TIMING EXPLORER; CYCLOTRON LINE; INTEGRAL OBSERVATION; A0535+262; ENERGY; RXTE; PERFORMANCE; LUMINOSITY; BINARIES; ORBIT AB We study the spectral and temporal behavior of the High Mass X-ray Binary A 0535+26 during a "pre-outburst flare" which took place similar to 5d before the peak of a normal (type I) outburst in August/September 2005. We compare the studied behavior with that observed during the outburst. Methods. We analyse RXTE observations that monitored A 0535+26 during the outburst. We complete spectral and timing analyses of the data. We study the evolution of the pulse period, present energy-dependent pulse profiles both at the initial pre-outburst flare and close to outburst maximum, and measure how the cyclotron resonance-scattering feature (hereafter CRSF) evolves. Results. We present three main results: a constant period P = 103.3960(5) s is measured until periastron passage, followed by a spin-up with a decreasing period derivative of. P = (-1.69 +/- 0.04) x 10(-8) s s(-1) at MJD 53 618, and P remains constant again at the end of the main outburst. The spin-up provides evidence for the existence of an accretion disk during the normal outburst. We measure a CRSF energy of E-cyc similar to 50 keV during the pre-outburst flare, and E-cyc similar to 46 keV during the main outburst. The pulse shape, which varies significantly during both pre-outburst flare and main outburst, evolves strongly with photon energy. C1 [Caballero, I.; Santangelo, A.; Staubert, R.; Postnov, K.; Klochkov, D.; Kreykenbohm, I.] Inst Astron & Astrophys, D-72076 Tubingen, Germany. [Kretschmar, P.] ESAC, ISOC, Madrid, Spain. [Postnov, K.] Moscow MV Lomonosov State Univ, Sternberg Astron Inst, Moscow 119992, Russia. [Camero-Arranz, A.] Univ Valencia, Inst Ciencias Mat, GACE, Valencia 46071, Spain. [Finger, M. H.; Wilson, C. A.] Natl Space Sci & Technol Ctr, Huntsville, AL 35805 USA. [Kreykenbohm, I.] ISDC, CH-1290 Versoix, Switzerland. [Pottschmidt, K.] Univ Maryland Baltimore Cty, CRESST, Baltimore, MD 21250 USA. [Pottschmidt, K.] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA. [Rothschild, R. E.; Suchy, S.] Univ Calif San Diego, CASS, La Jolla, CA 92093 USA. [Wilms, J.] Univ Erlangen Nurnberg, Astron Inst, D-96049 Bamberg, Germany. RP Caballero, I (reprint author), Inst Astron & Astrophys, Sand 1, D-72076 Tubingen, Germany. EM isabel@astro.uni-tuebingen.de RI Wilms, Joern/C-8116-2013; Kreykenbohm, Ingo/H-9659-2013; OI Wilms, Joern/0000-0003-2065-5410; Kreykenbohm, Ingo/0000-0001-7335-1803; Kretschmar, Peter/0000-0001-9840-2048 NR 35 TC 23 Z9 23 U1 0 U2 2 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD MAR PY 2008 VL 480 IS 2 BP L17 EP U1 DI 10.1051/0004-6361:20079310 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 271RP UT WOS:000253806700001 ER PT J AU Cordiner, MA Cox, NLJ Trundle, C Evans, CJ Hunter, I Przybilla, N Bresolin, F Salama, F AF Cordiner, M. A. Cox, N. L. J. Trundle, C. Evans, C. J. Hunter, I. Przybilla, N. Bresolin, F. Salama, F. TI Detection of diffuse interstellar bands in M 31 SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE astrochemistry; galaxies : Local Group; galaxies : ISM; ISM : lines and bands; ISM : clouds; ISM : dust; extinction ID SMALL-MAGELLANIC-CLOUD; ULTRAVIOLET EXTINCTION; CA-II; M31; SPECTROSCOPY; DUST; SUPERGIANTS; ABSORPTION; STARS; GAS AB Aims. We investigate the diffuse interstellar band (DIB) spectrum in the interstellar medium of M31. Methods. The DEIMOS spectrograph of the W. M. Keck observatory was used to make optical spectroscopic observations of two supergiant stars, MAG 63885 and MAG 70817, in the vicinity of the OB78 association in M 31 where the metallicity is approximately equal to solar. Results. The lambda lambda 5780, 5797, 6203, 6283 and 6613 DIBs are detected in both sightlines at velocities matching the M31 interstellar Na I absorption. The spectra are classified and interstellar reddenings are derived for both stars. Diffuse interstellar band ( DIB) equivalent widths and radial velocities are presented. Conclusions. The spectrum of DIBs observed in M31 towards MAG 63885 is found to be similar to that observed in the Milky Way. Towards MAG 70817 the DIB equivalent widths per unit reddening are about three times the Galactic average. Compared to observations elsewhere in the Universe, relative to reddening the M31 ISM in the vicinity of OB78 is apparently a highly favourable environment for the formation of DIB carriers. C1 [Cordiner, M. A.; Trundle, C.; Hunter, I.] Queens Univ Belfast, Sch Math & Phys, Astrophys Res Ctr, Belfast BT7 1NN, Antrim, North Ireland. [Cox, N. L. J.] ESA, Herschel Sci Ctr, European Space Astron Ctr, Madrid, Spain. [Evans, C. J.] Royal Observ, UK ATC, Edinburgh EH9 3HJ, Midlothian, Scotland. [Przybilla, N.] Dr Remeis Sternwarte Bamberg, D-96049 Bamberg, Germany. [Bresolin, F.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. [Salama, F.] NASA, Ames Res Ctr, Div Space Sci, Moffett Field, CA 94035 USA. RP Cordiner, MA (reprint author), Queens Univ Belfast, Sch Math & Phys, Astrophys Res Ctr, Belfast BT7 1NN, Antrim, North Ireland. EM m.cordiner@qub.ac.uk RI Salama, Farid/A-8787-2009 OI Salama, Farid/0000-0002-6064-4401 NR 45 TC 22 Z9 23 U1 0 U2 2 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD MAR PY 2008 VL 480 IS 1 BP L13 EP L16 DI 10.1051/0004-6361:20079309 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 268JP UT WOS:000253576400004 ER PT J AU Besson, DZ Jenkins, J Matsuno, S Nam, J Smith, M Barwick, SW Beatty, JJ Binns, WR Chen, C Chen, P Clem, JM Connolly, A Dowkontt, PF DuVernois, MA Field, RC Goldstein, D Gorham, PW Goodhue, A Hast, C Hebert, CL Hoover, S Israel, MH Kowalski, J Learned, JG Liewer, KM Link, JT Lusczek, E Mercurio, B Miki, C Miocinovic, P Naudet, CJ Ng, J Nichol, R Palladino, K Reil, K Romero-Wolf, A Rosen, M Ruckman, L Saltzberg, D Seckel, D Varner, GS Walz, D Wu, F AF Besson, D. Z. Jenkins, J. Matsuno, S. Nam, J. Smith, M. Barwick, S. W. Beatty, J. J. Binns, W. R. Chen, C. Chen, P. Clem, J. M. Connolly, A. Dowkontt, P. F. DuVernois, M. A. Field, R. C. Goldstein, D. Gorham, P. W. Goodhue, A. Hast, C. Hebert, C. L. Hoover, S. Israel, M. H. Kowalski, J. Learned, J. G. Liewer, K. M. Link, J. T. Lusczek, E. Mercurio, B. Miki, C. Miocinovic, P. Naudet, C. J. Ng, J. Nichol, R. Palladino, K. Reil, K. Romero-Wolf, A. Rosen, M. Ruckman, L. Saltzberg, D. Seckel, D. Varner, G. S. Walz, D. Wu, F. TI In situ radioglaciological measurements near Taylor Dome, Antarctica and implications for ultra-high energy (UHE) neutrino astronomy SO ASTROPARTICLE PHYSICS LA English DT Article DE ultra-high energy neutrino detection; radioglaciology; askaryan effect ID ICE SHEETS AB Radiowave detection of the Cherenkov radiation produced by neutrino-ice collisions requires an understanding of the radiofrequency (RF) response of cold polar ice. We herein report on a series of radioglaciological measurements performed approximately 10 km north of Taylor Dome Station, Antarctica from December 6, 2006-December 16, 2006. Using RF signals broadcast from: (a) an englacial discone, submerged to a depth of 100 m and broadcasting to a surface dual-polarization horn receiver, and (b) a dual-polarization horn antenna on the surface transmitting signals which reflect off the underlying bed and back up to the surface receiver, we have made time-domain estimates of both the real (index-of-refraction "n") and imaginary (attenuation length "L-atten") components of the complex ice dielectric constant. We have also measured the uniformity of ice response along two orthogonal axes in the horizontal plane. We observe an apparent wavespeed asymmetry of order 0.1% between two orthogonal linear polarizations projected into the horizontal plane, consistent with some previous measurements, but somewhat lower than others. (C) 2008 Elsevier B.V. All rights reserved. C1 [Besson, D. Z.; Link, J. T.] Univ Kansas, Dept Phys & Astron, Lawrence, KS 66045 USA. [Matsuno, S.; Gorham, P. W.; Hebert, C. L.; Kowalski, J.; Learned, J. G.; Miki, C.; Miocinovic, P.; Romero-Wolf, A.; Rosen, M.; Ruckman, L.; Varner, G. S.] Univ Hawaii Manoa, Dept Phys & Astron, Honolulu, HI 96822 USA. [Nam, J.; Barwick, S. W.; Goldstein, D.; Wu, F.] Univ Calif Irvine, Irvine, CA 92697 USA. [Beatty, J. J.; Mercurio, B.; Nichol, R.; Palladino, K.] Ohio State Univ, Dept Phys, Columbus, OH 43210 USA. [Binns, W. R.; Dowkontt, P. F.; Israel, M. H.] Washington Univ, Dept Phys, St Louis, MO 63130 USA. [Chen, C.; Chen, P.; Field, R. C.; Hast, C.; Ng, J.; Reil, K.; Walz, D.] Stanford Linear Accelerator Ctr, Menlo Pk, CA 94025 USA. [Clem, J. M.; Seckel, D.] Univ Delaware, Newark, DE 19716 USA. [Connolly, A.; Goodhue, A.; Hoover, S.; Saltzberg, D.] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA. [Lusczek, E.] Univ Minnesota, Sch Phys & Astron, Minneapolis, MN 55455 USA. [DuVernois, M. A.; Liewer, K. M.; Naudet, C. J.] Jet Propuls Lab, Pasadena, CA 91109 USA. RP Besson, DZ (reprint author), Univ Kansas, Dept Phys & Astron, Lawrence, KS 66045 USA. EM dbesson@ku.edu RI Nichol, Ryan/C-1645-2008; Vieregg, Abigail/D-2287-2012; Connolly, Amy/J-3958-2013; Beatty, James/D-9310-2011; OI Beatty, James/0000-0003-0481-4952; Lusczek, Elizabeth/0000-0003-4680-965X NR 29 TC 12 Z9 12 U1 0 U2 4 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0927-6505 J9 ASTROPART PHYS JI Astropart Phys. PD MAR PY 2008 VL 29 IS 2 BP 130 EP 157 DI 10.1016/j.astropartphys.2007.12.004 PG 28 WC Astronomy & Astrophysics; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA 280UO UT WOS:000254452100006 ER PT J AU Bruhweiler, F Verner, E AF Bruhweiler, F. Verner, E. TI Modeling Fe II emission and revised Fe II (UV) empirical templates SO ASTROPHYSICAL JOURNAL LA English DT Article DE line : formation; methods : numerical; quasars : emission lines; quasars : individual (I Zw 1); ultraviolet : galaxies ID ACTIVE GALACTIC NUCLEI; HIGH-REDSHIFT QUASARS; FLUORESCENCE LINES; BROAD EMISSION; RR TELESCOPII; IRON EMISSION; O-VI; ZW 1; SPECTRUM; RATIOS AB We use the narrow-lined broad-line region (BLR) of the Seyfert 1 galaxy, IZw 1, as a laboratory for modeling the ultraviolet (UV) Fe II 2100-3050 angstrom emission complex. We calculate a grid of Fe II emission spectra representative of BLR clouds and compare them with the observed I Zw 1 spectrum. Our predicted spectrum for log n(H)/(cm(-3)) = 11.0, log [Phi(H)/(cm(-2) s(-1)) = 20.5, and xi/( 1 km s(-1)) 20, using Cloudy and an 830 level model atom for Fe II with energies up to 14.06 eV, gives a better fit to the UV Fe II emission than models with fewer levels. Our analysis indicates ( 1) the observed UV Fe II emission must be corrected for an underlying Fe II pseudocontinuum; ( 2) Fe II emission peaks can be misidentified as that of other ions in active galactic nuclei ( AGNs) with narrow-lined BLRs possibly affecting deduced physical parameters; ( 3) the shape of 4200-4700 angstrom Fe II emission in I Zw 1 and other AGNs is a relative indicator of narrow-line region ( NLR) and BLR Fe II emission; ( 4) predicted ratios of Ly alpha, C III], and Fe II emission relative to Mg II lambda 2800 agree with extinction corrected observed I Zw1 fluxes, except for C IV lambda 1549; ( 5) the sensitivity of Fe II emission strength to microturbulence xi casts doubt on existing relative Fe/Mg abundances derived from Fe II ( UV)/Mg II flux ratios. Our calculated Fe II emission spectra, suitable for BLRs in AGNs, are available at http://iacs.cua.edu/people/verner/FeII. C1 [Bruhweiler, F.; Verner, E.] Catholic Univ Amer, Dept Phys, Inst Astrophys & Computat Sci, Washington, DC 20064 USA. [Bruhweiler, F.; Verner, E.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Bruhweiler, F (reprint author), Catholic Univ Amer, Dept Phys, Inst Astrophys & Computat Sci, 200 Hannan Hall, Washington, DC 20064 USA. EM bruhweiler@cua.edu; verner@milkyway.gsfc.nasa.gov NR 44 TC 32 Z9 33 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 MAR 1 PY 2008 VL 675 IS 1 BP 83 EP 95 DI 10.1086/525557 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 268EP UT WOS:000253562000008 ER PT J AU Sani, E Risaliti, G Salvati, M Maiolino, R Marconi, A Berta, S Braito, V Della Ceca, R Franceschini, A AF Sani, E. Risaliti, G. Salvati, M. Maiolino, R. Marconi, A. Berta, S. Braito, V. Della Ceca, R. Franceschini, A. TI 3-5 mu m spectroscopy of obscured AGNs in ULIRGs SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : active; galaxies : starburst; infrared : galaxies ID ULTRALUMINOUS INFRARED GALAXIES; ACTIVE GALACTIC NUCLEUS; OPTICAL SPECTROSCOPY; ENERGY-DISTRIBUTIONS; X-RAY; SAMPLE; SUPERANTENNAE; MICRON; QUASAR; ICE AB We present the results of infrared L-band (3-4 mu m) and M-band (4-5 mu m) Very Large Telescope (VLT) ISAAC spectroscopy of five bright ultraluminous infrared galaxies (ULIRGs) hosting an AGN. From our analysis we distinguish two types of sources: ULIRGs in which the AGN is unobscured ( with a flat continuum and no absorption features at 3.4 and 4.6 mu m), and those with highly obscured AGNs ( with a steep, reddened continuum and absorption features due to hydrocarbons and CO). Starburst activity is also present in all of the sources, as inferred from the 3.3 mu m PAH emission line. A strong correlation is found between continuum slope and CO optical depth, which suggests that deep carbon monoxide absorption is a common feature of highly obscured ULIRG AGNs. Finally, we show that the AGN dominates the 3-4 mu m emission, even if its contribution to the bolometric luminosity is small. C1 [Sani, E.; Marconi, A.] Univ Florence, Dipartimento Astron, I-50125 Florence, Italy. [Risaliti, G.; Salvati, M.] INAF Osservatorio Astron Roma, I-50125 Florence, Italy. [Risaliti, G.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Maiolino, R.] INAF Osservatorio Astron Roma, I-00040 Monte Porzio Catone, Italy. [Berta, S.; Franceschini, A.] Univ Padua, Dipartimento Astron, I-35122 Padua, Italy. [Braito, V.] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA. [Braito, V.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Della Ceca, R.] INAF Osservatorio Astron Brena, I-20121 Milan, Italy. RP Sani, E (reprint author), Univ Florence, Dipartimento Astron, Largo E Fremi 2, I-50125 Florence, Italy. RI Marconi, Alessandro/C-5880-2009; OI Marconi, Alessandro/0000-0002-9889-4238; Della Ceca, Roberto/0000-0001-7551-2252 NR 42 TC 24 Z9 24 U1 0 U2 1 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 MAR 1 PY 2008 VL 675 IS 1 BP 96 EP 105 DI 10.1086/523784 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 268EP UT WOS:000253562000009 ER PT J AU Bonamente, M Joy, M LaRoque, SJ Carlstrom, JE Nagai, D Marrone, DP AF Bonamente, Massimiliano Joy, Marshall LaRoque, Samuel J. Carlstrom, John E. Nagai, Daisuke Marrone, Daniel P. TI Scaling relations from Sunyaev-Zel'dovich effect and Chandra X-ray measurements of high-redshift galaxy clusters SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : clusters : general ID COSMIC DISTANCE SCALE; MASS; GAS; CONSTRAINTS; COSMOLOGY; FRACTIONS; TELESCOPE; EVOLUTION; CONSTANT; MODELS AB We present Sunyaev-Zel'dovich Effect (SZE) scaling relations for 38 massive galaxy clusters at redshifts 0.14 <= z <= 0.89, observed with both the Chandra X-ray Observatory and the centimeter-wave SZE imaging system at the BIMA and OVRO interferometric arrays. An isothermal beta-model with the central 100 kpc excluded from the X-ray data is used to model the intracluster medium and to measure global cluster properties. For each cluster, we measure the X-ray spectroscopic temperature, SZE gas mass, total mass, and integrated Compton y-parameters within r(2500). Our measurements are in agreement with the expectations based on a simple self-similar model of cluster formation and evolution. We compare the cluster properties derived from our SZE observations with and without Chandra spatial and spectral information and find them to be in good agreement. We compare our results with cosmological numerical simulations and find that simulations that include radiative cooling, star formation, and feedback match well both the slope and normalization of our SZE scaling relations. C1 [Bonamente, Massimiliano] Univ Alabama, Dept Phys, Huntsville, AL 35812 USA. [Bonamente, Massimiliano; Joy, Marshall] NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA. [LaRoque, Samuel J.; Carlstrom, John E.; Marrone, Daniel P.] Univ Chicago, Dept Astron & Astrophys, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA. [Carlstrom, John E.] Univ Chicago, Enrico Fermi Inst, Dept Phys, Chicago, IL 60637 USA. [Nagai, Daisuke] CALTECH, Pasadena, CA 91125 USA. Univ Alabama, Ctr Space Plasma & Aeron Res, Space Plasma Interact Data Anal & Simulat Lab, Huntsville, AL 35812 USA. RP Bonamente, M (reprint author), Univ Alabama, Dept Phys, Huntsville, AL 35812 USA. NR 47 TC 80 Z9 80 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAR 1 PY 2008 VL 675 IS 1 BP 106 EP 114 DI 10.1086/525517 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 268EP UT WOS:000253562000010 ER PT J AU Dessart, L Blondin, S Brown, PJ Hicken, M Hillier, DJ Holland, ST Immler, S Kirshner, RP Milne, P Modjaz, M Roming, PWA AF Dessart, Luc Blondin, Stephane Brown, Peter J. Hicken, Malcolm Hillier, D. John Holland, Stephen T. Immler, Stefan Kirshner, Robert P. Milne, Peter Modjaz, Maryam Roming, Peter W. A. TI Using quantitative spectroscopic analysis to determine the properties and distances of type II plateau supernovae: SN 2005cs and SN 2006bp SO ASTROPHYSICAL JOURNAL LA English DT Review DE radiative transfer; stars : atmospheres; stars : distances; stars : evolution; supernovae : individual (2005cs, 2006bp) ID EXPANDING PHOTOSPHERE METHOD; CORE-COLLAPSE SUPERNOVAE; X-RAY-EMISSION; PRELIMINARY SPECTRAL-ANALYSIS; LARGE-MAGELLANIC-CLOUD; LIGHT-CURVE; PLANETARY-NEBULAE; STANDARD CANDLES; CEPHEID DISTANCE; HUBBLE CONSTANT AB We analyze the Type II plateau supernovae (SNe IIP) SN 2005cs and SN 2006bp with the non-LTE model atmosphere code CMFGEN. We fit 13 spectra in the first month for SN 2005cs and 18 for SN 2006bp. Swift ultraviolet photometry and ground-based optical photometry calibrate each spectrum. Our analysis shows that both objects were discovered less than 3 days after they exploded, making these the earliest SN IIP spectra ever studied. They reveal broad and very weak lines from highly ionized fast ejecta with an extremely steep density profile. We identify He II lambda 4686 emission in the SN 2006bp ejecta. Days later, the spectra resemble the prototypical Type IIP SN 1999em, which had a supergiant-like photospheric composition. Despite the association of SN 2005cs with possible X-ray emission, the emergent UV and optical light comes from the photosphere, not from circumstellar emission. We surmise that the very steep density falloff we infer at early times may be a fossil of the combined actions of the shock wave passage and radiation driving at shock breakout. Based on tailored CMFGEN models, the direct fitting technique and the expanding photosphere method both yield distances and explosion times that agree within a few percent. We derive a distance to NGC 5194, the host of SN 2005cs, of 8.9 +/- 0.5 Mpc and 17.5 +/- 0.8 Mpc for SN 2006bp in NGC 3953. The luminosity of SN 2006bp is 1.5 times that of SN 1999em and 6 times that of SN 2005cs. Reliable distances to SNe IIP that do not depend on a small range in luminosity provide an independent route to the Hubble constant and improved constraints on other cosmological parameters. C1 [Dessart, Luc; Milne, Peter] Univ Arizona, Dept Astron, Tucson, AZ 85721 USA. [Dessart, Luc; Milne, Peter] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Blondin, Stephane; Hicken, Malcolm; Kirshner, Robert P.; Modjaz, Maryam] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 01238 USA. [Brown, Peter J.; Roming, Peter W. A.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Hillier, D. John] Univ Pittsburgh, Dept Phys & Astron, Pittsburgh, PA 15260 USA. [Holland, Stephen T.; Immler, Stefan] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Xray Astrophys Branch, Greenbelt, MD 20771 USA. [Hillier, D. John; Holland, Stephen T.] Univ Space Res Assoc, Columbia, MD 21044 USA. RP Dessart, L (reprint author), Univ Arizona, Dept Astron, Tucson, AZ 85721 USA. EM luc@as.arizona.edu NR 102 TC 80 Z9 80 U1 0 U2 1 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 MAR 1 PY 2008 VL 675 IS 1 BP 644 EP 669 DI 10.1086/526451 PG 26 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 268EP UT WOS:000253562000049 ER PT J AU Tuthill, PG Monnier, JD Lawrance, N Danchi, WC Owocki, SP Gayley, KG AF Tuthill, Peter G. Monnier, John D. Lawrance, Nicholas Danchi, William C. Owocki, Stan P. Gayley, Kenneth G. TI The prototype colliding-wind pinwheel WR 104 SO ASTROPHYSICAL JOURNAL LA English DT Article DE instrumentation : interferometers; stars : imaging; stars : individual (WR 104); stars : mass loss; stars : winds, outflows ID WOLF-RAYET STARS; SUDDEN RADIATIVE BRAKING; KECK APERTURE-MASKING; MASSIVE STARS; DUST FORMATION; BINARY WR-140; X-RAY; INTERFEROMETRY; EVOLUTION; BURST AB Results from the most extensive study of the time-evolving dust structure around the prototype "pinwheel'' nebula WR 104 are presented. Encompassing 11 epochs in three near-infrared filter bandpasses, a homogeneous imaging data set spanning more than 6 yr (or 10 orbits) is presented. Data were obtained from the highly successful Keck Aperture Masking Experiment, which can recover high-fidelity images at extremely high angular resolutions, revealing the geometry of the plume with unprecedented precision. Inferred properties for the (unresolved) underlying binary and wind system are orbital period 241.5 +/- 0.5 days and angular outflow velocity 0.28 +/- 0.02 mas day(-1). An optically thin cavity of angular size 13.3 +/- 1.4 mas was found to lie between the central binary and the onset of the spiral dust plume. Rotational motion of the wind system induced by the binary orbit is found to have important ramifications: entanglement of the winds results in strong shock activity far downstream from the nose of the bow shock. The far greater fraction of the winds participating in the collision may play a key role in gas compression and the nucleation of dust at large radii from the central binary and shock stagnation point. Investigation of the effects of radiative braking points toward significant modifications of the simple hydrostatic colliding wind geometry, extending the relevance of this phenomenon to wider binary systems than previously considered. Limits placed on the maximum allowed orbital eccentricity of e less than or similar to 0.06 argue strongly for a prehistory of tidal circularization in this system. Finally, we discuss the implications of Earth's polar (i less than or similar to 16 degrees) vantage point onto a system likely to host supernova explosions at future epochs. C1 [Tuthill, Peter G.] Univ Sydney, Sch Phys, Sydney, NSW 2006, Australia. [Monnier, John D.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Lawrance, Nicholas] Univ Sydney, Sch Aerosp Mech & Mechatron Engn, Sydney, NSW 2006, Australia. [Danchi, William C.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Owocki, Stan P.] Univ Delaware, Bartol Res Inst, Newark, DE 19716 USA. [Gayley, Kenneth G.] Univ Iowa, Iowa City, IA 52245 USA. RP Tuthill, PG (reprint author), Univ Sydney, Sch Phys, Sydney, NSW 2006, Australia. EM p.tuthill@physics.usyd.edu.au; monnier@umich.edu; n.lawrance@acfr.usyd.edu.au; wcd@iri1.gsfc.nasa.gov; owocki@bartol.udel.edu; ken.gayley@gmail.com NR 75 TC 46 Z9 46 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 MAR 1 PY 2008 VL 675 IS 1 BP 698 EP 710 DI 10.1086/527286 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 268EP UT WOS:000253562000053 ER PT J AU Rhee, JH Song, I Zuckerman, B AF Rhee, Joseph H. Song, Inseok Zuckerman, B. TI Warm dust in the terrestrial planet zone of a Sun-like pleiades star: Collisions between planetary embryos? SO ASTROPHYSICAL JOURNAL LA English DT Article DE circumstellar matter; infrared : stars; open clusters and associations : individual (Pleiades) planetary systems : formation; stars : individual (HD 23514) ID DEBRIS DISKS; HIPPARCOS; ORIGIN; PLANETESIMALS; SPECTROGRAPH; MAGNITUDE; EVOLUTION; ASTEROIDS; HD-69830; DIAGRAMS AB Only a few solar-type main-sequence stars are known to be orbited by warm dust particles; the most extreme is the G0 field star BD + 20 307 that emits similar to 4% of its energy at mid-infrared wavelengths. We report the identification of a similarly dusty star HD 23514, an F6-type member of the Pleiades. A strong mid-IR silicate emission feature indicates the presence of small warm dust particles, but with the primary flux density peak at the nonstandard wavelength of similar to 9 mu m. The existence of so much dust within an AU or so of these stars is not easily accounted for given the very brief lifetime in orbit of small particles. The apparent absence of very hot (greater than or similar to 1000 K) dust at both stars suggests the possible presence of a planet closer to the stars than the dust. The observed frequency of the BD + 20 307/HD 23514 phenomenon indicates that the mass equivalent of Earth's Moon must be converted, via collisions of massive bodies, to tiny dust particles that find their way to the terrestrial planet zone during the first few hundred million years of the life of many (most?) Sun-like stars. Identification of these two dusty systems among youthful nearby solar-type stars suggests that terrestrial planet formation is common. C1 [Rhee, Joseph H.; Zuckerman, B.] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA. [Song, Inseok] CALTECH, IPAC, Spitzer Sci Ctr, Pasadena, CA 91125 USA. [Zuckerman, B.] NASA, Astrobiol Inst, Washington, DC 20546 USA. RP Rhee, JH (reprint author), Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA. EM rhee@astro.ucla.edu; song@ipac.caltech.edu; ben@astro.ucla.edu NR 48 TC 57 Z9 57 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 MAR 1 PY 2008 VL 675 IS 1 BP 777 EP 783 DI 10.1086/524935 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 268EP UT WOS:000253562000058 ER PT J AU Sheeley, NR Herbst, AD Palatchi, CA Wang, YM Howard, RA Moses, JD Vourlidas, A Newmark, JS Socker, DG Plunkett, SP Korendyke, CM Burlaga, LF Davila, JM Thompson, WT St Cyr, OC Harrison, RA Davis, CJ Eyles, CJ Halain, JP Wang, D Rich, NB Battams, K Esfandiari, E Stenborg, G AF Sheeley, N. R. Herbst, A. D. Palatchi, C. A. Wang, Y. -M. Howard, R. A. Moses, J. D. Vourlidas, A. Newmark, J. S. Socker, D. G. Plunkett, S. P. Korendyke, C. M. Burlaga, L. F. Davila, J. M. Thompson, W. T. St Cyr, O. C. Harrison, R. A. Davis, C. J. Eyles, C. J. Halain, J. P. Wang, D. Rich, N. B. Battams, K. Esfandiari, E. Stenborg, G. TI Heliospheric images of the solar wind at Earth SO ASTROPHYSICAL JOURNAL LA English DT Article DE Sun : corona; Sun : coronal mass ejections (CMEs); Sun : magnetic fields ID CORONAL MASS EJECTIONS AB During relatively quiet solar conditions throughout the spring and summer of 2007, the SECCHI HI2 white-light telescope on the STEREO B solar-orbiting spacecraft observed a succession of wave fronts sweeping past Earth. We have compared these heliospheric images with in situ plasma and magnetic field measurements obtained by near-Earth spacecraft, and we have found a near perfect association between the occurrence of these waves and the arrival of density enhancements at the leading edges of high-speed solar wind streams. Virtually all of the strong corotating interaction regions are accompanied by large-scale waves, and the low-density regions between them lack such waves. Because the Sun was dominated by long-lived coronal holes and recurrent solar wind streams during this interval, there is little doubt that we have been observing the compression regions that are formed at low latitude as solar rotation causes the high-speed wind from coronal holes to run into lower speed wind ahead of it. C1 [Sheeley, N. R.; Palatchi, C. A.; Wang, Y. -M.; Howard, R. A.; Moses, J. D.; Vourlidas, A.; Newmark, J. S.; Socker, D. G.; Plunkett, S. P.; Korendyke, C. M.] USN, Res Lab, Div Space Sci, Washington, DC 20375 USA. [Burlaga, L. F.; Davila, J. M.; Thompson, W. T.; St Cyr, O. C.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20742 USA. [Harrison, R. A.; Davis, C. J.] Rutherford Appleton Lab, Didcot OX11 OQX, Oxon, England. [Eyles, C. J.] Univ Birmingham, Sch Phys & Astron, Birmingham B15 2TT, W Midlands, England. [Halain, J. P.] Univ Liege, Ctr Spatiale Liege, B-4031 Angleur, Belgium. [Wang, D.; Rich, N. B.; Battams, K.; Esfandiari, E.] Interferometr Inc, Herndon, VA 20171 USA. [Stenborg, G.] Catholic Univ Amer, Washington, DC 20064 USA. RP Sheeley, NR (reprint author), USN, Res Lab, Div Space Sci, Washington, DC 20375 USA. EM sheeley@spruce.nrl.navy.mil RI Vourlidas, Angelos/C-8231-2009; Thompson, William/D-7376-2012; Scott, Christopher/H-8664-2012 OI Vourlidas, Angelos/0000-0002-8164-5948; Scott, Christopher/0000-0001-6411-5649 NR 12 TC 91 Z9 92 U1 1 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 MAR 1 PY 2008 VL 675 IS 1 BP 853 EP 862 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 268EP UT WOS:000253562000064 ER PT J AU Lis, DC Bockelee-Morvan, D Boissier, J Crovisier, J Biver, N Charnley, SB AF Lis, D. C. Bockelee-Morvan, D. Boissier, J. Crovisier, J. Biver, N. Charnley, S. B. TI Hydrogen isocyanide in comet 73P/Schwassmann-Wachmann (fragment B) SO ASTROPHYSICAL JOURNAL LA English DT Article DE comets : individual (73P/Schwassmann-Wachmann); molecular processes; radio lines : solar system ID C1 IKEYA-ZHANG; SPECTROSCOPIC OBSERVATIONS; HNC; HCN; ABUNDANCES; HYAKUTAKE; CHEMISTRY; SPECTRUM; U90.7; LEE AB We present a sensitive 3 sigma upper limit of 1.1% for the HNC/HCN abundance ratio in comet 73P/SchwassmannWachmann (fragment B), obtained on 2006 May 10-11, using Caltech Submillimeter Observatory (CSO). This limit is a factor of similar to 7 lower than the values measured previously in moderately active comets at 1 AU from the Sun. Comet 73P/Schwassmann-Wachmann was depleted in most volatile species, except of HCN. The low HNC/HCN ratio thus argues against HNC production from polymers produced from HCN. However, thermal degradation of macromolecules, or polymers, produced from ammonia and carbon compounds, such as acetylene, methane, or ethane appears a plausible explanation for the observed variations of the HNC/HCN ratio in moderately active comets, including the very low ratio in comet 73P/Schwassmann-Wachmann reported here. Similar polymers have been invoked previously to explain anomalous N-14/N-15 ratios measured in cometary CN. C1 [Lis, D. C.] CALTECH, Down Lab Phys 320 47, Pasadena, CA 91125 USA. [Lis, D. C.] LESIA Observ, Paris, France. [Boissier, J.; Crovisier, J.; Biver, N.] Observ Paris, CNRS, UMR 8109, F-92195 Meudon, France. [Boissier, J.; Crovisier, J.; Biver, N.] LESIA, F-92195 Meudon, France. [Charnley, S. B.] NASA, Ames Res Ctr, Space Sci & Astrobiol Div, Moffett Field, CA 94035 USA. RP Lis, DC (reprint author), CALTECH, Down Lab Phys 320 47, Pasadena, CA 91125 USA. EM dcl@caltech.edu; Dominique.Bockelee@obspm.fr; Jeremie.Boissier@obspm.fr; Jacques.Crovisier@obspm.fr; Nicolas.Biver@obspm.fr; charnley@dusty.arc.nasa.gov RI Charnley, Steven/C-9538-2012 NR 44 TC 24 Z9 24 U1 2 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 MAR 1 PY 2008 VL 675 IS 1 BP 931 EP 936 DI 10.1086/527345 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 268EP UT WOS:000253562000072 ER PT J AU Dorodnitsyn, A Kallman, T Proga, D AF Dorodnitsyn, A. Kallman, T. Proga, D. TI An axisymmetric, hydrodynamical model for the torus wind in active galactic nuclei SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE acceleration of particles; galaxies : active; hydrodynamics; methods : numerical; quasars : absorption lines; X-rays : galaxies ID X-RAY BINARIES; SEYFERT-GALAXIES; ANGULAR-MOMENTUM; IONIZED-GAS; ENVIRONMENT; NGC-1068; NGC-3783 AB We report on time-dependent axisymmetric simulations of an X-ray-excited flow from a parsec-scale, rotating, cold torus around an active galactic nucleus. Our simulations account for radiative heating and cooling and radiation pressure force. The simulations follow the development of a broad biconical outflow induced mainly by X-ray heating. We compute synthetic spectra predicted by our simulations. The wind characteristics and the spectra support the hypothesis that a rotationally supported torus can serve as the source of a wind which is responsible for the warm absorber gas observed in the X-ray spectra of many Seyfert galaxies. C1 [Dorodnitsyn, A.] NASA, Goddard Space Flight Ctr, High Energy Astrophys Lab, Greenbelt, MD 20771 USA. [Kallman, T.] Moscow Space Res Inst, Moscow 117997, Russia. [Proga, D.] Univ Nevada, Dept Phys & Astron, Las Vegas, NV 89154 USA. RP Dorodnitsyn, A (reprint author), NASA, Goddard Space Flight Ctr, High Energy Astrophys Lab, Code 662, Greenbelt, MD 20771 USA. NR 20 TC 18 Z9 18 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD MAR 1 PY 2008 VL 675 IS 1 BP L5 EP L8 DI 10.1086/529374 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 291ZA UT WOS:000255234900002 ER PT J AU Shioya, Y Taniguchi, Y Sasaki, SS Nagao, T Murayama, T Takahashi, MI Ajiki, M Ideue, Y Mihara, S Nakajima, A Scoville, NZ Mobasher, B Aussel, H Giavalisco, M Guzzo, L Hasinger, G Impey, C Le Fevre, O Lilly, S Renzini, A Rich, M Sanders, DB Schinnerer, E Shopbell, P Leauthaud, A Kneib, JP Rhodes, J Massey, R AF Shioya, Y. Taniguchi, Y. Sasaki, S. S. Nagao, T. Murayama, T. Takahashi, M. I. Ajiki, M. Ideue, Y. Mihara, S. Nakajima, A. Scoville, N. Z. Mobasher, B. Aussel, H. Giavalisco, M. Guzzo, L. Hasinger, G. Impey, C. Le Fevre, O. Lilly, S. Renzini, A. Rich, M. Sanders, D. B. Schinnerer, E. Shopbell, P. Leauthaud, A. Kneib, J. -P. Rhodes, J. Massey, R. TI The H alpha luminosity function and star formation rate at z approximate to 0.24 in the COSMOS 2 square degree field SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE galaxies : distances and redshifts; galaxies : evolution; galaxies : luminosity function, mass function ID GALAXY REDSHIFT SURVEY; SUBARU DEEP FIELD; LYMAN BREAK GALAXIES; NONTHERMAL RADIO-EMISSION; FORMATION RATE DENSITY; NEUTRAL GAS GALAXIES; NORMAL DISK GALAXIES; DIGITAL SKY SURVEY; FORMATION HISTORY; FORMING GALAXIES AB To derive a new H alpha luminosity function and to understand the clustering properties of star-forming galaxies at z approximate to 0.24, we have made a narrowband imaging survey for H alpha-emitting galaxies in the Hubble Space Telescope (HST) COSMOS 2 square degree field. We used the narrowband filter NB816 (lambda(c) = 8150 angstrom, Delta lambda = 120 angstrom) and sampled H alpha emitters with EW(obs)(H alpha + [N II]) > 12 angstrom in a redshift range between z = 0.233 and 0.251 corresponding to a depth of 70 Mpc. We obtained 980 H alpha-emitting galaxies in a sky area of 5540 arcmin(2), corresponding to a survey volume of 3.1 x 10(4) Mpc(3). We derive a H alpha luminosity function with a best-fit Schechter function parameter set of alpha=-1.35(-0.13)(+0.11), log phi* = -2.65(-0.38)(+0.27), and L*(ergs s(-1)) = 41.94(-0.23)(+0.38). The H alpha luminosity density is 2.7(-0.6)(+0.7) x 10(39) ergs s(-1) Mpc(-3). After subtracting the AGN contribution ( 15%) to the H alpha luminosity density, the star formation rate density is evaluated as 1.8(-0.4)(+0.7) x 10(-2) M(circle dot) yr(-1) Mpc(-3). The angular two-point correlation function of H alpha-emitting galaxies of log L(H alpha) > 39.8 is well fit by a power-law form of w(theta) = 0.013(-0.001)(+0.002)theta(-0.88 +/- 0.03) , corresponding to the correlation function of xi(r) = (r/1.9 Mpc)(-1.88). We also find that the H alpha emitters with higher H alpha luminosity are more strongly clustered than those with lower luminosity. C1 [Shioya, Y.; Taniguchi, Y.] Ehime Univ, Res Ctr Space & Cosm Evolut, Matsuyama, Ehime 7908577, Japan. [Sasaki, S. S.; Ideue, Y.; Mihara, S.; Nakajima, A.] Ehime Univ, Grad Sch Sci & Engn, Matsuyama, Ehime 7908577, Japan. [Sasaki, S. S.; Murayama, T.; Takahashi, M. I.; Ajiki, M.] Tohoku Univ, Astron Inst, Grad Sch Sci, Aoba Ku, Sendai, Miyagi 9808578, Japan. [Sasaki, S. S.; Scoville, N. Z.; Shopbell, P.; Kneib, J. -P.; Rhodes, J.; Massey, R.] CALTECH, Dept Astron, Pasadena, CA 91125 USA. [Nagao, T.] Natl Inst Nat Sci, Natl Astron Observ Japan, Mitaka, Tokyo 1818588, Japan. [Scoville, N. Z.; Aussel, H.; Sanders, D. B.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. [Mobasher, B.; Giavalisco, M.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Aussel, H.] CEA Saclay, DSM DAPNIA SAp, F-91191 Gif Sur Yvette, France. [Guzzo, L.] Osserv Astron Brera, Milan, Italy. [Hasinger, G.] Max Planck Inst Extraterr Phys, D-85478 Garching, Germany. [Impey, C.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Le Fevre, O.; Leauthaud, A.; Kneib, J. -P.] Lab Astrophys Marseille, F-13376 Marseille 12, France. [Lilly, S.] ETH, Dept Phys, Swiss Fed Inst Technol, CH-8093 Zurich, Switzerland. [Renzini, A.] European So Observ, D-85748 Garching, Germany. [Rich, M.] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA. [Schinnerer, E.] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Massey, R.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Shioya, Y (reprint author), Ehime Univ, Res Ctr Space & Cosm Evolut, Bunkyo Cho, Matsuyama, Ehime 7908577, Japan. RI Le Fevre, Olivier/G-7389-2011; Kneib, Jean-Paul/A-7919-2015 OI Kneib, Jean-Paul/0000-0002-4616-4989 NR 88 TC 52 Z9 53 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0067-0049 J9 ASTROPHYS J SUPPL S JI Astrophys. J. Suppl. Ser. PD MAR PY 2008 VL 175 IS 1 BP 128 EP 137 DI 10.1086/523703 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 307CO UT WOS:000256295600008 ER PT J AU Sakamoto, T Barthelmy, SD Barbier, L Cummings, JR Fenimore, EE Gehrels, N Hullinger, D Krimm, HA Markwardt, CB Palmer, DM Parsons, AM Sato, G Stamatikos, M Tueller, J Ukwatta, TN Zhang, B AF Sakamoto, T. Barthelmy, S. D. Barbier, L. Cummings, J. R. Fenimore, E. E. Gehrels, N. Hullinger, D. Krimm, H. A. Markwardt, C. B. Palmer, D. M. Parsons, A. M. Sato, G. Stamatikos, M. Tueller, J. Ukwatta, T. N. Zhang, B. TI The first Swift bat gamma-ray burst catalog SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE gamma rays : bursts ID X-RAY; TELESCOPE; AFTERGLOW; SPECTRUM; FLASHES; MISSION; HARD AB We present the first Swift Burst Alert Telescope (BAT) catalog of gamma-ray bursts (GRBs), which contains bursts detected by the BAT between 2004 December 19 and 2007 June 16. This catalog (hereafter the BAT1 catalog) contains burst trigger time, location, 90% error radius, duration, fluence, peak flux, and time-averaged spectral parameters for each of 237 GRBs, as measured by the BAT. The BAT-determined position reported here is within 1.75' of the Swift X-Ray Telescope (XRT)-determined position for 90% of these GRBs. The BAT T-90 and T-50 durations peak at 80 and 20 s, respectively. From the fluence-fluence correlation, we conclude that about 60% of the observed peak energies, E-peak(obs), of BAT GRBs could be less than 100 keV. We confirm that GRB fluence to hardness and GRB peak flux to hardness are correlated for BAT bursts in analogous ways to previous missions' results. The correlation between the photon index in a simple power-law model and E-peak(obs) is also confirmed. We also report the current status for the on-orbit BAT calibrations based on observations of the Crab Nebula. C1 [Sakamoto, T.; Barthelmy, S. D.; Barbier, L.; Cummings, J. R.; Gehrels, N.; Krimm, H. A.; Markwardt, C. B.; Parsons, A. M.; Sato, G.; Stamatikos, M.; Tueller, J.; Ukwatta, T. N.] NASA, Goddard Space Flight Ctr, CRESST, Greenbelt, MD 20771 USA. [Sakamoto, T.; Stamatikos, M.] Oak Ridge Associated Univ, Oak Ridge, TN 37831 USA. [Cummings, J. R.] Univ Maryland, Joint Ctr Astrophys, Baltimore, MD 21250 USA. [Fenimore, E. E.; Palmer, D. M.] Los Alamos Natl Lab, Los Alamos, NM 87545 USA. [Hullinger, D.] Moxtek Inc, Orem, UT 84057 USA. [Krimm, H. A.] Univ Space Res Assoc, Columbia, MD 21044 USA. [Markwardt, C. B.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Sato, G.] Japan Aerosp Explorat Agcy, Inst Space & Astronaut Sci, Sagamihara, Kanagawa 2298510, Japan. [Ukwatta, T. N.] George Washington Univ, Dept Phys, Ctr Nucl Studies, Washington, DC 20052 USA. [Zhang, B.] Univ Nevada, Dept Phys & Astron, Las Vegas, NV 89154 USA. RP Sakamoto, T (reprint author), NASA, Goddard Space Flight Ctr, CRESST, Greenbelt, MD 20771 USA. RI Barthelmy, Scott/D-2943-2012; Gehrels, Neil/D-2971-2012; Tueller, Jack/D-5334-2012; Parsons, Ann/I-6604-2012 NR 28 TC 117 Z9 119 U1 0 U2 2 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0067-0049 J9 ASTROPHYS J SUPPL S JI Astrophys. J. Suppl. Ser. PD MAR PY 2008 VL 175 IS 1 BP 179 EP 190 DI 10.1086/523646 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 307CO UT WOS:000256295600012 ER PT J AU Hains, JC Taubman, BF Thompson, AM Stehr, JW Marufu, LT Doddridge, BG Dickerson, RR AF Hains, Jennifer C. Taubman, Brett F. Thompson, Anne M. Stehr, Jeffrey W. Marufu, Lackson T. Doddridge, Bruce G. Dickerson, Russell R. TI Origins of chemical pollution derived from Mid-Atlantic aircraft profiles using a clustering technique SO ATMOSPHERIC ENVIRONMENT LA English DT Article DE ozone; SO2; clustering; emissions ID SYNOPTIC METEOROLOGICAL CONTROLS; LIGHT-SCATTERING CHARACTERISTICS; VERTICAL TRANSPORT PROCESSES; AIR-QUALITY MODELS; TROPOSPHERIC OZONE; RELATIVE-HUMIDITY; PRECIPITATION CHEMISTRY; PARTICULATE MATTER; BACK TRAJECTORIES; UNITED-STATES AB Upwind sources of NOx and SO2 play a crucial role in the amount of O-3 and aerosols in the lower troposphere in the Mid-Atlantic US. This paper describes a novel method of clustering trace gas and aerosol profiles allowing for the quantification of the relationship between point sources and pollution levels. This improves our understanding of pollution origins and has the potential for prediction of episodes of poor air quality. A hierarchical clustering method was used to classify distinct chemical and meteorological events from over 200 aircraft vertical profiles in the lower troposphere. Profile measurements included O-3, SO2, CO and particle scattering from June to August 1997-2003, in the Mid-Atlantic US (mostly in Maryland, Pennsylvania and Virginia). The clustering technique could discriminate distinct profile shapes including measurements made during the 2002 Canadian forest fires. Forty-eight-hour back trajectories were run for each profile and the integrated NOx and SO2 point source emissions encountered by each trajectory were calculated using data from the EPA Clean Air Market Division's emissions database. There was a strong correlation between integrated NOx emissions and O-3 profiles, indicating that O-3 profiles are strongly influenced by and can be predicted with point source emissions. There is a prevalent concentration of SO2 over the eastern US with mixing ratios decreasing smoothly from about 3.5 ppb near the surface to 0.2 ppb at 2400 m. (C) 2007 Elsevier Ltd. All rights reserved. C1 [Hains, Jennifer C.; Dickerson, Russell R.] Univ Maryland, Dept Chem, College Pk, MD 20742 USA. [Taubman, Brett F.] Appalachian State Univ, Dept Chem, Boone, NC 28608 USA. [Dickerson, Russell R.] Penn State Univ, Dept Meteorol, University Pk, PA 16802 USA. [Stehr, Jeffrey W.] Univ Maryland, Dept Atmospher Ocean & Space Sci, College Pk, MD 20742 USA. [Marufu, Lackson T.; Doddridge, Bruce G.] NASA, Langley Res Ctr, Hampton, VA USA. RP Hains, JC (reprint author), Univ Maryland, Dept Chem, College Pk, MD 20742 USA. EM hains@knmi.nl RI Stehr, Jeffrey/F-2638-2010; Dickerson, Russell/F-2857-2010; Thompson, Anne /C-3649-2014 OI Stehr, Jeffrey/0000-0003-4840-6942; Dickerson, Russell/0000-0003-0206-3083; Thompson, Anne /0000-0002-7829-0920 NR 45 TC 31 Z9 31 U1 1 U2 13 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 1352-2310 J9 ATMOS ENVIRON JI Atmos. Environ. PD MAR PY 2008 VL 42 IS 8 BP 1727 EP 1741 DI 10.1016/j.atmosenv.2007.11.052 PG 15 WC Environmental Sciences; Meteorology & Atmospheric Sciences SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences GA 284SO UT WOS:000254726300006 ER PT J AU Jordan, NS Ichoku, C Hoff, RM AF Jordan, Nikisa S. Ichoku, Charles Hoff, Raymond M. TI Estimating smoke emissions over the US Southern Great Plains using MODIS fire radiative power and aerosol observations SO ATMOSPHERIC ENVIRONMENT LA English DT Article DE fire radiative energy (FRE); smoke; MODIS; emissions ID BIOMASS BURNING EMISSIONS; IMAGING SPECTRORADIOMETER MODIS; OPTICAL-PROPERTIES; EOS-MODIS; SATELLITE; ENERGY; PARTICLES; PRODUCTS; SYSTEM; LAND AB A newly developed method, which involves the use of satellite measurements of energy released by fires, was used to estimate smoke emissions in the United States (US) Southern Great Plains (SGP). This SGP region was chosen because extensive agricultural and planned burning occurs there annually. Moderate resolution imaging spectroradiometer (MODIS) aerosol optical depth (AOD) and fire radiative energy (FRE) release rates (R-FRF), acquired in 2004 from the Terra and Aqua satellites, were used to derive a FRE-based smoke emission coefficient (C-e kgMJ(-1)), which when multiplied by R-FRE (MJs(-1)) gives the rate of smoke emission (kg s(-1)). Correlations between the smoke emission rates and the RFRE were significant for Terra-MODIS (R-2 = 0.645, n = 146, p < 0.0001) and Aqua-MODIS (R-2 = 0.752, n = 178, p < 0.0001). Furthermore, the C, values derived independently from Terra and Aqua were in close agreement, and the average C, for this area is 0.049 +/- 0.024 kg MJ(-1). A Monte Carlo (MC) probabilistic approach was used to approximate uncertainties from the smoke emission and resulting C,. For the first time, smoke emission estimates have been derived for the US SGP using observations of energy released by fires. Although more work is necessary, the present study demonstrates the feasibility of using RFRE for smoke emission estimation in that region. Burning peaked during the spring and fall seasons. Moreover, qualitative examination of smoke emission patterns side-by-side with local air-quality measurements indicated that the impact of smoke from local biomass burning activities was significant on the regional airquality. (c) 2008 Elsevier Ltd. All rights reserved. C1 [Jordan, Nikisa S.; Hoff, Raymond M.] Univ Maryland, Joint Ctr Earth Syst Technol JCET, Cooperat Ctr Remote Sensing Sci & Technol CREST, Baltimore, MD 21250 USA. [Ichoku, Charles] Univ Maryland, ESSIC, College Pk, MD 20742 USA. [Ichoku, Charles] NASA, Goddard Space Flight Ctr, Climate & Radiat Branch, Greenbelt, MD 20771 USA. RP Jordan, NS (reprint author), Univ Maryland, Joint Ctr Earth Syst Technol JCET, Cooperat Ctr Remote Sensing Sci & Technol CREST, Baltimore Cty 5523,Res Pk Dr,Suite 320, Baltimore, MD 21250 USA. EM njordan1@umbc.edu RI Hoff, Raymond/C-6747-2012; Ichoku, Charles/E-1857-2012 OI Ichoku, Charles/0000-0003-3244-4549 NR 61 TC 20 Z9 20 U1 3 U2 9 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 1352-2310 EI 1873-2844 J9 ATMOS ENVIRON JI Atmos. Environ. PD MAR PY 2008 VL 42 IS 9 BP 2007 EP 2022 DI 10.1016/j.atmosenv.2007.12.023 PG 16 WC Environmental Sciences; Meteorology & Atmospheric Sciences SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences GA 297MM UT WOS:000255620800005 ER PT J AU Civerolo, KL Hogrefe, C Lynn, B Rosenzweig, C Goldberg, R Rosenthal, J Knowlton, K Kinney, PL AF Civerolo, Kevin L. Hogrefe, Christian Lynn, Barry Rosenzweig, Cynthia Goldberg, Richard Rosenthal, Joyce Knowlton, Kim Kinney, Patrick L. TI Simulated effects of climate change on summertime nitrogen deposition in the eastern US SO ATMOSPHERIC ENVIRONMENT LA English DT Article DE atmospheric deposition; climate change; CMAQ; MM5; nitrogen ID NORTHEASTERN UNITED-STATES; COMMUNITY MULTISCALE AIR; ATMOSPHERIC DEPOSITION; ACIDIC DEPOSITION; DRY DEPOSITION; TRENDS NETWORK; MODEL; QUALITY; INVENTORY; EMISSIONS AB It is anticipated that climate change may impact regional-scale air quality and atmospheric deposition in the coming decades. To simulate the effects of climate change on nitrogen (N) deposition across numerous watersheds in the eastern US, we applied the NASA Goddard Institute for Space Studies General Circulation Model (GISS-GCM), Fifth Generation Pennsylvania State University/National Center for Atmospheric Research Mesoscale Model (MM5), Sparse Matrix Operator Kernel Emissions (SMOKE) modeling system, and the US Environmental Protection Agency Community Multiscale Air Quality (CMAQ) Model. Keeping chemical initial and boundary conditions, land use, and anthropogenic area and point source emissions fixed, this modeling system was applied over five summers (June-August) from 1993 to 1997 and five summers from 2053 to 2057. Over these eastern US watersheds, the modeling system estimated 3-14% increases in summertime N deposition as a result of climate change. This increase is primarily due to the direct effects of climate change on atmospheric conditions and chemistry. Wet N deposition is predicted to increase as a result of increased precipitation, while dry N deposition is predicted to increase as higher surface temperatures favor gas-phase nitric acid to particulate nitrate. The simulated increase suggests that additional reductions in N oxides and/or ammonia may be needed to fully realize the anticipated benefits of planned reduction strategies, including the Clean Air Interstate Rule (CAIR). (c) 2007 Elsevier Ltd. All rights reserved. C1 [Civerolo, Kevin L.; Hogrefe, Christian] New York State Dept Environm Conservat, Div Air Resources, Albany, NY 12233 USA. [Hogrefe, Christian] SUNY Albany, Atmospher Sci Res Ctr, Albany, NY 12222 USA. [Lynn, Barry; Rosenzweig, Cynthia; Goldberg, Richard] NASA, Goddard Inst Space Studies, New York, NY 10025 USA. [Rosenthal, Joyce] Columbia Univ, Grad Sch Architecture Planning & Preservat, New York, NY USA. [Knowlton, Kim; Kinney, Patrick L.] Columbia Univ, Mailman Sch Publ Hlth, New York, NY USA. RP Civerolo, KL (reprint author), New York State Dept Environm Conservat, Div Air Resources, 625 Broadway, Albany, NY 12233 USA. EM kxcivero@gw.dec.state.ny.us RI Kinney, Patrick/H-7914-2012; OI Civerolo, Kevin/0000-0003-1536-2664 NR 40 TC 6 Z9 7 U1 0 U2 10 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 1352-2310 J9 ATMOS ENVIRON JI Atmos. Environ. PD MAR PY 2008 VL 42 IS 9 BP 2074 EP 2082 DI 10.1016/j.atmosenv.2007.11.049 PG 9 WC Environmental Sciences; Meteorology & Atmospheric Sciences SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences GA 297MM UT WOS:000255620800010 ER PT J AU Bhatia, AK Landi, E AF Bhatia, A. K. Landi, E. TI Atomic data and spectral line intensities for Ar XV SO ATOMIC DATA AND NUCLEAR DATA TABLES LA English DT Article ID BE-LIKE IONS; BERYLLIUM ISOELECTRONIC SEQUENCE; ELECTRON-IMPACT EXCITATION; COLLISION STRENGTHS; EMISSION-LINES; OSCILLATOR-STRENGTHS; RATE COEFFICIENTS; CROSS-SECTIONS; TRANSITIONS; NI AB Electron impact collision strengths, energy levels, oscillator strengths, and spontaneous radiative decay rates are calculated for Ar XV. The configurations used are 2s(2), 2s2p, 2p(2), 2l3l', 2l4l' and 2s5l', with l = s, p and l' = s, p, d giving rise to 92 fine-structure levels in intermediate coupling, Collision strengths are calculated at eight incident energies (10, 20, 30, 60, 120, 180, 240, and 300 Ry) for transitions within the three lowest configurations, and five incident energies (60, 120, 180, 240, and 300 Ry) for transitions between the lowest five levels and the n = 3, 4, 5 configurations, using the distorted wave approximation. Excitation rate coefficients are calculated as a function of electron temperature by assuming a Maxwellian electron velocity distribution. Using the excitation rate coefficients and the radiative transition rates of the present work, and R-matrix results for the 2s(2), 2s2p, 2P(2) configurations available in the literature, statistical equilibrium equations for level populations are solved at electron densities covering the range of 10(8)-10(14) cm(-3) at an electron temperature of log T-e(K) = 6.6, corresponding to the maximum abundance of Ar XV. Spectral line intensities are calculated, and their diagnostic relevance is discussed. Observed line ratios indicate electron temperatures of the relevant emitting plasma close to log T-e(K) = 6.6. This dataset will be made available in the next version of the CHIANTI database. (C) 2007 Elsevier Inc. All rights reserved. C1 [Landi, E.] USN, Res Lab, Washington, DC 20375 USA. [Bhatia, A. K.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Landi, E.] ARTEP Inc, Columbia, MD 21044 USA. RP Landi, E (reprint author), USN, Res Lab, Washington, DC 20375 USA. EM Landi@poppeo.nrl.navy.mil RI Landi, Enrico/H-4493-2011 NR 31 TC 7 Z9 7 U1 0 U2 2 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0092-640X J9 ATOM DATA NUCL DATA JI Atom. Data Nucl. Data Tables PD MAR PY 2008 VL 94 IS 2 BP 223 EP 256 DI 10.1016/j.adt.2007.11.001 PG 34 WC Physics, Atomic, Molecular & Chemical; Physics, Nuclear SC Physics GA 274JW UT WOS:000253998600002 ER PT J AU Le Marshall, J Jung, J Zapotocny, T Redder, C Dunn, M Daniels, J Riishojgaard, LP AF Le Marshall, J. Jung, J. Zapotocny, T. Redder, C. Dunn, M. Daniels, J. Riishojgaard, Lars Peter TI Impact of MODIS atmospheric motion vectors on a global NWP system SO AUSTRALIAN METEOROLOGICAL MAGAZINE LA English DT Article ID DATA ASSIMILATION SYSTEM; POLAR-REGIONS; CLOUD-DRIFT; WINDS C1 [Le Marshall, J.; Jung, J.; Zapotocny, T.; Redder, C.; Dunn, M.; Daniels, J.; Riishojgaard, Lars Peter] Joint Ctr Satellite Data Assimilat, Camp Springs, MD USA. [Jung, J.; Zapotocny, T.] CIMSS, Madison, WI USA. [Redder, C.; Riishojgaard, Lars Peter] Global Modeling Assimilat Off, NASA GSFC, Greenbelt, MD USA. [Dunn, M.] La Trobe Univ, Bundoora, Vic, Australia. [Daniels, J.] NOAA NESDIS STAR, Camp Springs, MD USA. RP Le Marshall, J (reprint author), Bur Meteorol, Ctr Australian Weather & Climate Res, GPO Box 1289, Melbourne, Vic 3001, Australia. EM j.lemarshall@bom.gov.au RI Daniels, Jaime/E-7933-2011 OI Daniels, Jaime/0000-0002-9438-6631 NR 19 TC 9 Z9 9 U1 0 U2 3 PU AUSTRALIAN BUREAU METEOROLOGY PI MELBOURNE PA GPO BOX 1289, MELBOURNE, VIC 3001, AUSTRALIA SN 0004-9743 J9 AUST METEOROL MAG JI Aust. Meteorol. Mag. PD MAR PY 2008 VL 57 IS 1 BP 45 EP 51 PG 7 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 318IL UT WOS:000257084700004 ER PT J AU Bornstein, BJ Keating, SM Jouraku, A Hucka, M AF Bornstein, Benjamin J. Keating, Sarah M. Jouraku, Akiya Hucka, Michael TI LibSBML: an API library for SBML SO BIOINFORMATICS LA English DT Article ID MODELS AB LibSBML is an application programming interface library for reading, writing, manipulating and validating content expressed in the Systems Biology Markup Language (SBML) format. It is written in ISO C and C++, provides language bindings for Common Lisp, Java, Python, Perl, MATLAB and Octave, and includes many features that facilitate adoption and use of both SBML and the library. Developers can embed libSBML in their applications, saving themselves the work of implementing their own SBML parsing, manipulation and validation software. C1 [Keating, Sarah M.; Hucka, Michael] CALTECH, Biol Network Modeling Ctr, Pasadena, CA 91125 USA. [Bornstein, Benjamin J.] NASA, Jet Propuls Lab, Washington, DC 20546 USA. [Jouraku, Akiya] Keio Univ, Sch Fundamental Sci & Technol, Yokohama, Kanagawa 223, Japan. RP Keating, SM (reprint author), CALTECH, Biol Network Modeling Ctr, Pasadena, CA 91125 USA. RI Hucka, Michael/B-1896-2012; OI Keating, Sarah/0000-0002-3356-3542 FU Biotechnology and Biological Sciences Research Council; NIGMS NIH HHS [R01 GM070923, R01 GM070923-04, R01 GM077671] NR 8 TC 135 Z9 137 U1 1 U2 7 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 1367-4803 J9 BIOINFORMATICS JI Bioinformatics PD MAR PY 2008 VL 24 IS 6 BP 880 EP 881 DI 10.1093/bioinformatics/btn051 PG 2 WC Biochemical Research Methods; Biotechnology & Applied Microbiology; Computer Science, Interdisciplinary Applications; Mathematical & Computational Biology; Statistics & Probability SC Biochemistry & Molecular Biology; Biotechnology & Applied Microbiology; Computer Science; Mathematical & Computational Biology; Mathematics GA 274OK UT WOS:000254010400026 PM 18252737 ER PT J AU Gu, L Hanson, PJ Mac Post, W Kaiser, DP Yang, B Nemani, R Pallardy, SG Meyers, T AF Gu, Lianhong Hanson, Paul J. Mac Post, W. Kaiser, Dale P. Yang, Bai Nemani, Ramakrishna Pallardy, Stephen G. Meyers, Tilden TI The 2007 eastern US spring freezes: Increased cold damage in a warming world? SO BIOSCIENCE LA English DT Article DE extreme temperature fluctuation; frost damage; plant phenology; climate warming; carbon cycle ID ELEVATED ATMOSPHERIC CO2; FROST HARDINESS; CLIMATE-CHANGE; WINTER THAW; RED SPRUCE; SCOTS PINE; GROWTH; TOLERANCE; INJURY; TREES AB Plant ecologists have long been concerned with a seemingly paradoxical scenario in the relationship between plant growth and climate change: warming may actually increase the risk of plant frost damage. The underlying hypothesis is that mild winters and warm, early springs, which are expected to occur as the climate warms, may induce premature plant development, resulting in exposure of vulnerable plant tissues and organs to subsequent late-season frosts. The 2007 spring freeze in the eastern United States provides an excellent opportunity to evaluate this hypothesis and assess its large-scale consequences. In this article, we contrast the rapid prefreeze phenological advancement caused by unusually warm conditions with the dramatic postfreeze setback, and report complicated patterns of freeze damage to plants. The widespread devastation of crops and natural vegetation occasioned by this event demonstrates the need to consider large fluctuations in spring temperatures a real threat to terrestrial ecosystem structure and functioning in a warming climate. C1 [Gu, Lianhong; Hanson, Paul J.; Mac Post, W.; Kaiser, Dale P.; Yang, Bai] Oak Ridge Natl Lab, Div Environm Sci, Oak Ridge, TN 37831 USA. [Nemani, Ramakrishna] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Pallardy, Stephen G.] Univ Missouri, Dept Forestry, Columbia, MO USA. [Meyers, Tilden] Natl Ocean Atmospher Adm, Air Resources Lab, Atmospher Turbulence & Diffus Div, Oak Ridge, TN USA. RP Gu, L (reprint author), Oak Ridge Natl Lab, Div Environm Sci, POB 2008, Oak Ridge, TN 37831 USA. EM lianhong-gu@ornl.gov RI Hanson, Paul J./D-8069-2011; Post, Wilfred/B-8959-2012; Meyers, Tilden/C-6633-2016; Gu, Lianhong/H-8241-2014 OI Hanson, Paul J./0000-0001-7293-3561; Gu, Lianhong/0000-0001-5756-8738 NR 38 TC 190 Z9 204 U1 8 U2 84 PU AMER INST BIOLOGICAL SCI PI WASHINGTON PA 1444 EYE ST, NW, STE 200, WASHINGTON, DC 20005 USA SN 0006-3568 J9 BIOSCIENCE JI Bioscience PD MAR PY 2008 VL 58 IS 3 BP 253 EP 262 DI 10.1641/B580311 PG 10 WC Biology SC Life Sciences & Biomedicine - Other Topics GA 275KQ UT WOS:000254070700011 ER PT J AU Smith, SM Zwart, SR Heer, M Lee, SMC Baecker, N Meuche, S Macias, BR Shackelford, LC Schneider, S Hargens, AR AF Smith, Scott M. Zwart, Sara R. Heer, Martina Lee, Stuart M. C. Baecker, Natalie Meuche, Sabine Macias, Brandon R. Shackelford, Linda C. Schneider, Suzanne Hargens, Alan R. TI WISE-2005: Supine treadmill exercise within lower body negative pressure and flywheel resistive exercise as a countermeasure to bed rest-induced bone loss in women during 60-day simulated microgravity SO BONE LA English DT Article DE bone turnover markers; exercise; space flight; bed rest; simulated weightlessness ID MUSCLE-FIBER FUNCTION; RESISTANCE EXERCISE; SPACE-FLIGHT; NUTRITIONAL-STATUS; UPRIGHT EXERCISE; CONCURRENT EXERCISE; IDENTICAL-TWINS; FOLLOW-UP; PAMIDRONATE; RESORPTION AB Bone loss associated with disuse during bed rest (BR), an analog of space flight, can be attenuated by exercise. In previous studies, the efficacy of either aerobic or resistive exercise countermeasures has been examined separately. We hypothesized that a regimen of combined resistive and aerobic exercise during BR would prevent bone resorption and promote bone formation. After a 20-day ambulatory adaptation to controlled confinement and diet, 16 women participated in a 60-day, 6 head-down-tilt BR and were assigned randomly to one of the two groups. Control subjects (CON, n=8) performed no countermeasure. Exercise subjects (EX, n=8) participated in an exercise program during BR, alternating between supine treadmill exercise within lower body negative pressure (3-4 d wk(-1)) and flywheel resistive exercise (2-3 d wk(-1)). By the last week of BR, excretion of helical peptide (CON, 79% +/- 44 increase; EX, 64% +/- 50, mean +/- SD) and N-terminal cross-linking telopeptide (CON, 51% +/- 34; EX, 43% +/- 56), markers of bone resorption, were greater than they were before BR in both groups (P<0.05). However, serum concentrations of the bone formation marker procollagen type I N propeptide were greater in EX than CON throughout and after bed rest (P<0.05), while concentrations of the bone formation marker bone alkaline phosphatase tended to be greater in EX than CON. Dual-energy X-ray absorptiometry results indicated that the exercise treatment significantly (P<0.05) attenuated loss of hip and leg bone mineral density in EX compared to CON. The combination of resistive and aerobic exercise did not prevent bone resorption but did promote bone formation, and helped mitigate the net bone loss associated with simulated microgravity. (c) 2007 Published by Elsevier Inc. C1 [Smith, Scott M.; Shackelford, Linda C.] NASA, Lyndon B Johnson Space Ctr, Nutr Biochem Lab,Natl Aeronaut & Space Adm, Human Adaptat & Countermeasures Div, Houston, TX 77058 USA. [Zwart, Sara R.] Univ Space Res Assoc, Houston, TX 77058 USA. [Heer, Martina; Baecker, Natalie] DLR, Inst Aerosp Med, Cologne, Germany. [Lee, Stuart M. C.] Wyle, Houston, TX 77058 USA. [Meuche, Sabine; Macias, Brandon R.; Hargens, Alan R.] Univ Calif San Diego, Med Ctr, Dept Orthopaed Surg, San Diego, CA 92103 USA. [Meuche, Sabine] Charite Univ Med Berlin, Ctr Space Med, D-13353 Berlin, Germany. [Schneider, Suzanne] Univ New Mexico, Dept Phys Performance & Dev, Albuquerque, NM 87131 USA. RP Smith, SM (reprint author), NASA, Lyndon B Johnson Space Ctr, Nutr Biochem Lab,Natl Aeronaut & Space Adm, Human Adaptat & Countermeasures Div, Mail Code SK3,2101 NASA Pkwy, Houston, TX 77058 USA. EM scott.m.smith@nasa.gov NR 41 TC 38 Z9 39 U1 1 U2 6 PU ELSEVIER SCIENCE INC PI NEW YORK PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA SN 8756-3282 J9 BONE JI Bone PD MAR PY 2008 VL 42 IS 3 BP 572 EP 581 DI 10.1016/j.bone.2007.11.015 PG 10 WC Endocrinology & Metabolism SC Endocrinology & Metabolism GA 271OW UT WOS:000253799500014 PM 18249055 ER PT J AU Anthes, RA Bernhardt, PA Chen, Y Cucurull, L Dymond, KF Ector, D Healy, SB Ho, SP Hunt, DC Kuo, YH Liu, H Manning, K Mccormick, C Meehan, TK Randel, WJ Rocken, C Schreiner, WS Sokolovskiy, SV Syndergaard, S Thompson, DC Trenberth, KE Wee, TK Yen, NL Zeng, Z AF Anthes, R. A. Bernhardt, P. A. Chen, Y. Cucurull, L. Dymond, K. F. Ector, D. Healy, S. B. Ho, S. -P. Hunt, D. C. Kuo, Y. -H. Liu, H. Manning, K. Mccormick, C. Meehan, T. K. Randel, W. J. Rocken, C. Schreiner, W. S. Sokolovskiy, S. V. Syndergaard, S. Thompson, D. C. Trenberth, K. E. Wee, T. -K. Yen, N. L. Zeng, Z. TI The COSMOC/FORMOSAT-3 - Mission early results SO BULLETIN OF THE AMERICAN METEOROLOGICAL SOCIETY LA English DT Article ID RADIO OCCULTATION MEASUREMENTS; GLOBAL POSITIONING SYSTEM; LOW-EARTH-ORBIT; COSMIC CONSTELLATION; TROPICAL TROPOPAUSE; LOWER TROPOSPHERE; ATMOSPHERE; INSTRUMENT; CLIMATE; SIGNALS AB The radio occultation (RO) technique, which makes use of radio signals transmitted by the global positioning system (GPS) satellites, has emerged as a powerful and relatively inexpensive approach for sounding the global atmosphere with high precision, accuracy, and vertical resolution in all weather and over both land and ocean. On 15 April 2006, the joint Taiwan-U.S. Constellation Observing System for Meteorology, Ionosphere, and Climate (COSMIC)/Formosa Satellite Mission 3 (COSMIC/FORMOSAT-3, hereafter COSMIC) mission, a constellation of six micro satellites, was launched into a 512-km orbit. After launch the satellites were gradually deployed to their final orbits at 800 km, a process that took about 17 months. During the early weeks of the deployment, the satellites were spaced closely, offering a unique opportunity to verify the high precision of RO measurements. As of September 2007, COSMIC is providing about 2000 RO soundings per day to support the research and operational communities. COSMIC RO data are of better quality than those from the previous missions and penetrate much farther down into the troposphere; 70%-90% of the soundings reach to within 1 km of the surface on a global basis. The data are having a positive impact oil operational global weather forecast models. With the ability to penetrate deep into the lower troposphere using an advanced open-loop tracking technique, the COSMIC RO instruments can observe the structure of the tropical atmospheric boundary layer. The value of RO for climate monitoring and research is demonstrated by the precise and consistent observations between different instruments, platforms, and missions. COSMIC observations are capable of intercalibrating microwave measurements from the Advanced Microwave Sounding Unit (AMSU) on different satellites. Finally, unique and useful observations of the ionosphere are being obtained using the RO receiver and two other instruments on the COSMIC satellites, the tiny ionosphere photometer (TIP) and the tri-band beacon. C1 [Cucurull, L.; Ector, D.; Ho, S. -P.; Hunt, D. C.; Kuo, Y. -H.; Rocken, C.; Schreiner, W. S.; Sokolovskiy, S. V.; Syndergaard, S.; Wee, T. -K.; Zeng, Z.] Univ Corp Atmospher Res, Boulder, CO USA. [Bernhardt, P. A.; Dymond, K. F.] Naval Res Lab, Washington, DC USA. [Chen, Y.; Ho, S. -P.; Liu, H.; Manning, K.; Randel, W. J.; Trenberth, K. E.] Natl Ctr Atmospher Res, Boulder, CO 80307 USA. [Healy, S. B.] European Ctr Medium Range Weather Forecasts, Reading RG2 9AX, Berks, England. [Meehan, T. K.] Jet Prop Lab, Pasadena, CA USA. [Thompson, D. C.] Utah State Univ, Logan, UT 84322 USA. [Yen, N. L.] Natl Space Org, Hsinchu, Taiwan. RP Kuo, YH (reprint author), UCAR, POB 3000, Boulder, CO 80307 USA. EM kuo@ucar.edu RI Trenberth, Kevin/A-5683-2012; Zeng, Zhen/J-5183-2014; Cucurull, Lidia/E-8900-2015; Randel, William/K-3267-2016; Syndergaard, Stig/C-1103-2017 OI Trenberth, Kevin/0000-0002-1445-1000; Randel, William/0000-0002-5999-7162; Syndergaard, Stig/0000-0003-3119-2618 NR 59 TC 375 Z9 392 U1 6 U2 44 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 0003-0007 EI 1520-0477 J9 B AM METEOROL SOC JI Bull. Amer. Meteorol. Soc. PD MAR PY 2008 VL 89 IS 3 BP 313 EP 333 DI 10.1175/BAMS-89-3-313 PG 21 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 286MA UT WOS:000254848800013 ER PT J AU Lau, KM Ramanathan, V Wu, GX Li, Z Tsay, SC Hsu, C Sikka, R Holben, B Lu, D Tartari, G Chin, M Koudelova, R Chen, H Ma, Y Huang, J Taniguchi, K Zhang, R AF Lau, K. -M. Ramanathan, V. Wu, G. -X. Li, Z. Tsay, S. C. Hsu, C. Sikka, R. Holben, B. Lu, D. Tartari, G. Chin, M. Koudelova, R. Chen, H. Ma, Y. Huang, J. Taniguchi, K. Zhang, R. TI The Joint Aerosol-Monsoon Experiment - A new challenge for monsoon climate research SO BULLETIN OF THE AMERICAN METEOROLOGICAL SOCIETY LA English DT Article ID ATMOSPHERIC BROWN CLOUDS; TIBETAN PLATEAU; CLOUDINESS; REDUCTION; POLLUTION; RAINFALL; IMPACTS; NETWORK; INDIA; CHINA AB Aerosol- and moonsoon-related droughts and floods are two of the most serious environmental hazards confronting more than 60% of the population of the world living in the Asian monsoon countries. In recent years, thanks to improved satellite and in situ observations, and better models, great strides have been made in aerosol and monsoon research, respectively. There is now a growing body of evidence suggesting that interaction of aerosol forcing with monsoon dynamics may alter the redistribution of energy in the atmosphere and at the Earth's surface, thereby influencing monsoon water cycle and climate. In this article, the authors describe the scientific rationale and challenges for an integrated approach to study the interactions between aerosol and monsoon water cycle dynamics. A joint Aerosol-Monsoon Experiment (JAMEX) is proposed for 2007-11, with enhanced observations of the physical and chemical properties, sources and sinks, and long-range transport of aerosols, in conjunction with meteorological and oceanographic observations in the Indo-Pacific continental and oceanic regions. JAMEX will leverage on coordination among many ongoing and planned national research programs on aerosols and monsoons in China, India, Japan, Nepal, Italy, and the United States, as well as international research programs of the World Climate Research Program (WCRP) and the World Meteorological Organization (WMO). C1 [Lau, K. -M.; Tsay, S. C.; Hsu, C.; Chin, M.] NASA, Goddard Space Flight Ctr, Atmospheres Lab, Greenbelt, MD 20771 USA. [Ramanathan, V.] Univ Calif San Diego, Ctr Clouds Chem & Climate, Scripps Inst Oceanog, La Jolla, CA 92093 USA. [Wu, G. -X.] Chinese Acad Sci, Inst Atmospher Phys, State Key Lab Atmosphere Sci & Geophys Fluid Dyna, Beijing, Peoples R China. [Li, Z.] Univ Maryland, Dept Atmospher & Ocean Sci, College Pk, MD 20742 USA. [Holben, B.] NASA, Goddard Space Flight Ctr, Lab Hydrosphere, Greenbelt, MD 20771 USA. [Tartari, G.] CNR, Water Res Inst, Milan, Italy. [Tartari, G.] EV K2 CNR Comm, Bergamo, Italy. [Koudelova, R.] Univ Tokyo, CEOP Int Project Off, Tokyo, Japan. [Ma, Y.] Chinese Acad Sci, Inst Tibetan Plateau Res, Beijing, Peoples R China. [Huang, J.] Lanzhou Univ, Sch Atmospher Sci, Lanzhou 730000, Peoples R China. [Taniguchi, K.] Univ Tokyo, Dept Civil Engn, Tokyo 113, Japan. [Zhang, R.] Chinese Acad Sci, Inst Atmospher Phys, Beijing, Peoples R China. RP Lau, KM (reprint author), NASA, Goddard Space Flight Ctr, Atmospheres Lab, Greenbelt, MD 20771 USA. EM William.K.Lau@nasa.gov RI Chin, Mian/J-8354-2012; Hsu, N. Christina/H-3420-2013; Li, Zhanqing/F-4424-2010; Tsay, Si-Chee/J-1147-2014; Taniguchi, Kenji/C-3429-2015; Lau, William /E-1510-2012 OI Li, Zhanqing/0000-0001-6737-382X; Lau, William /0000-0002-3587-3691 NR 36 TC 122 Z9 128 U1 2 U2 29 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 0003-0007 EI 1520-0477 J9 B AM METEOROL SOC JI Bull. Amer. Meteorol. Soc. PD MAR PY 2008 VL 89 IS 3 BP 369 EP + DI 10.1175/BAMS-89-3-369 PG 16 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 286MA UT WOS:000254848800016 ER PT J AU Manderson, JP AF Manderson, John P. TI The spatial scale of phase synchrony in winter flounder (Pseudopleuronectes americanus) production increased among southern New England nurseries in the 1990s SO CANADIAN JOURNAL OF FISHERIES AND AQUATIC SCIENCES LA English DT Article ID SHRIMP CRANGON-SEPTEMSPINOSA; NORTHEASTERN US ESTUARIES; POPULATION-DYNAMICS; ENVIRONMENTAL NOISE; NARRAGANSETT BAY; CLIMATE-CHANGE; PREDATION; HABITAT; GROWTH; LARVAE AB The spatial scales at which the dynamics of subpopulations are synchronized affect regional population persistence and reflect the operational spatial scales of factors regulating populations. I examined phase synchrony in the fluctuations of age-0 winter flounder (Pseudopleuronectes americanus) production among 19 southern New England (SNE), USA, coastal nurseries. From 1990 to 2004, nursery production was synchronized at scales up to similar to 200 km based on spatial trends in cross-correlations of first-differenced age-0 abundance time series. However, sliding window analysis of 1975-2005 time series collected in six nurseries <= 55 km apart in northern SNE indicated that synchrony increased from low to high values in the early 1990s. Synchrony in production also increased among three nurseries <= 65 km apart in southern SNE from 1984 to 2004. Thus, interannual fluctuations in nursery production appeared to become synchronized at coarser spatial scales throughout SNE during the 1990s. This coarsening of the spatial scale of control of winter flounder nursery production was coincident with an increase in the frequency of springs with warm temperatures believed to negatively affect early life history processes. Spatial synchronization of winter flounder nursery ground production could destabilize the age-class structure and population dynamics in the region. C1 NOAA, Natl Marine Fisheries Serv, Ecosyst Proc Div, Behav Ecol Branch,James J Howard Marine Sci Lab, Highlands, NJ 07732 USA. RP Manderson, JP (reprint author), NOAA, Natl Marine Fisheries Serv, Ecosyst Proc Div, Behav Ecol Branch,James J Howard Marine Sci Lab, 74 Magruder Rd, Highlands, NJ 07732 USA. EM john.manderson@noaa.gov NR 54 TC 17 Z9 18 U1 2 U2 9 PU NATL RESEARCH COUNCIL CANADA-N R C RESEARCH PRESS PI OTTAWA PA BUILDING M 55, OTTAWA, ON K1A 0R6, CANADA SN 0706-652X J9 CAN J FISH AQUAT SCI JI Can. J. Fish. Aquat. Sci. PD MAR PY 2008 VL 65 IS 3 BP 340 EP 351 DI 10.1139/F07-169 PG 12 WC Fisheries; Marine & Freshwater Biology SC Fisheries; Marine & Freshwater Biology GA 271FT UT WOS:000253775000002 ER PT J AU Vertrees, RA Zwischenberger, JB Boor, PJ Popov, V McCarthy, M Solley, TN Goodwin, TJ AF Vertrees, Roger A. Zwischenberger, Joseph B. Boor, Paul J. Popov, Vselovod McCarthy, Maureen Solley, Travis N. Goodwin, Thomas J. TI Cellular differentiation in three-dimensional lung cell cultures SO CANCER BIOLOGY & THERAPY LA English DT Article DE tissue engineering; lung cells; co-culture ID EPITHELIAL MEMBRANE ANTIGEN; MUCIN GENE-EXPRESSION; III BETA-TUBULIN; MONOCLONAL-ANTIBODIES; IN-VITRO; SQUAMOUS DIFFERENTIATION; VONWILLEBRAND-FACTOR; MESENCHYMAL CELLS; BASEMENT-MEMBRANE; CARCINOMA CELLS AB Introduction: Aspects of human biology that are not sufficiently addressed by current cell culture models are cellular differentiation and three-dimensional ( 3-D) structural organization. A model that more closely associates the presence and biology of organelles to molecular expressions relevant to these organelles may provide evidence of cellular differentiation and the beginning steps in the construction of a 3-D architecture. The development of a new model-3-D cell cultures-may ultimately provide a better understanding of lung biology and pathobiology. Purpose: The purpose of this study was to develop both traditional monolayer and 3-D cell cultures of a known and well documented normal lung cell line and then to determine similarities and differences between these cultures in terms of differentiation and molecular marker expression. Results: Electron microscopy identified presence of lipid inclusion, microvilli, extra cellular matrix, and tight junctions in the 3-D cultures; differentiation not seen in ML cultures. The degree of differentiation determined by immunohistochemistry when the cell line was grown as ML or 3-D cultures shows that ultra-structure and marker expressions were more representative of control tissue than when cells were grown in 3-D than as MLs. Methods: An immortalized cell line was grown as a traditional monolayer ( ML) in culture flasks and as 3-D cultures in rotating walled vessels and incubated under identical conditions. Comparison for presence of differentiation and marker expression between these cultures and control tissue collected from surgical patient specimens was studied. Electron microscopy for identification of ultra structures, and immunohistochemistry ( ZO-1, EMA, ICAM-1, villin, tubulin, CK 18, VWF, Collagen IV and human mucin) for phenotypic comparisons between cells in ML and 3-D cell cultures was conducted. Summary: The development of 3-D cell cultures will provide for a new and more powerful tool in the study of lung biology and pathobiology. C1 [Vertrees, Roger A.; Solley, Travis N.] Univ Texas Med Branch, Dept Surg, Galveston, TX 77555 USA. [Boor, Paul J.; Popov, Vselovod] Univ Texas Med Branch, Dept Pathol, Galveston, TX 77555 USA. [Zwischenberger, Joseph B.] Univ Kentucky, Dept Surg, Lexington, KY USA. [McCarthy, Maureen] NASA, Lyndon B Johnson Space Ctr, Univ Space Res Assoc, Houston, TX 77058 USA. [Goodwin, Thomas J.] NASA, Lyndon B Johnson Space Ctr, Dis Modelling Tissue Analogues Lab, Houston, TX 77058 USA. RP Vertrees, RA (reprint author), Univ Texas Med Branch, Dept Surg, 301 Univ Blvd, Galveston, TX 77555 USA. EM rvertree@utmb.edu NR 69 TC 1 Z9 1 U1 0 U2 1 PU LANDES BIOSCIENCE PI AUSTIN PA 1806 RIO GRANDE ST, AUSTIN, TX 78702 USA SN 1538-4047 J9 CANCER BIOL THER JI Cancer Biol. Ther. PD MAR PY 2008 VL 7 IS 3 BP 405 EP U7 PG 8 WC Oncology SC Oncology GA 312HB UT WOS:000256658700016 ER PT J AU Bishop, JL Lane, MD Dyar, MD Brown, AJ AF Bishop, J. L. Lane, M. D. Dyar, M. D. Brown, A. J. TI Reflectance and emission spectroscopy study of four groups of phyllosilicates: smectites, kaolinite-serpentines, chlorites and micas SO CLAY MINERALS LA English DT Article DE spectroscopy; reflectance; emissivity; smectite; kaolinite; serpentine; chlorite; mica ID SOCIETY SOURCE CLAYS; BASE-LINE; INFRARED-SPECTROSCOPY; DIOCTAHEDRAL SMECTITES; MINERALS; MARS; SPECTRA; DISSOLUTION; CELADONITE; CALIFORNIA AB Coordinated visible/near-infrared reflectance/mid-infrared reflectance and emissivity spectra of four groups of phyllosilicates were undertaken to provide insights into the differences within and among groups of smectites, kaolinite-serpentines, chlorites and micas. Identification and characterization of phyllosilicates via remote sensing on Earth and Mars can be achieved using the OH combination bands in the 2.2-2.5 mu m region and the tetrahedral SiO4 vibrations from similar to 8.8-12 mu m (similar to 1140-830 cm(-1)) and similar to 20-25 mu m (500-400 cm(-1)). The sharp and well resolved OH combination bands in the 2.2-2.5 mu m region provide unique fingerprints for specific minerals. Al-rich phyllosilicates exhibit OH combination bands near 2.2 mu m, while these bands are observed near 2.29-2.31, 2.33-2.34 mu m and near 2.35-2.37 mu m for Fe3+-rich, Mg-rich and Fe2+-rich phyllosilicates, respectively. When a tetrahedral substitution of Al or Fe3+ for Si occurs, the position of the Si(Al,Fe)O-4 stretching mode absorption shifts. Depending on the size of the cation, the Si(Al,Fe)O-4 bending mode near 500 cm(-1) is split into multiple bands that may be distinguished via hyperspectral remote sensing techniques. The tetrahedral SiO4 vibrations are also influenced by the octahedral cations, such that Al-rich, Fe-rich and Mg-rich phyllosilicates can be discriminated in reflectance and emissivity spectra based on diagnostic positions of the stretching and bending bands. Differences among formation conditions for these four groups of phyllosilicates are also discussed. Hyperspectral remote sensing can be used to identify specific phyllosilicates using electronic and vibrational features and thus provide constraints on the chemistry and formation conditions of soils. C1 [Bishop, J. L.; Brown, A. J.] NASA, Ames Res Ctr, SETI Inst, Mountain View, CA 94043 USA. [Lane, M. D.] Planetary Sci Inst, Tucson, AZ 85719 USA. [Dyar, M. D.] Mt Holyoke Coll, S Hadley, MA 01075 USA. RP Bishop, JL (reprint author), NASA, Ames Res Ctr, SETI Inst, 515 N Whisman Rd, Mountain View, CA 94043 USA. EM jbishop@mail.arc.nasa.gov NR 60 TC 126 Z9 126 U1 10 U2 36 PU MINERALOGICAL SOC PI TWICKENHAM PA 12 BAYLIS MEWS, AMYAND PARK ROAD,, TWICKENHAM TW1 3HQ, MIDDLESEX, ENGLAND SN 0009-8558 EI 1471-8030 J9 CLAY MINER JI Clay Min. PD MAR PY 2008 VL 43 IS 1 BP 35 EP 54 DI 10.1180/claymin.2008.043.1.03 PG 20 WC Chemistry, Physical; Geosciences, Multidisciplinary; Mineralogy SC Chemistry; Geology; Mineralogy GA 289GP UT WOS:000255043300003 ER PT J AU Bishop, JL Dyar, MD Sklute, EC Drief, A AF Bishop, J. L. Dyar, M. D. Sklute, E. C. Drief, A. TI Physical alteration of antigorite: a Mossbauer spectroscopy, reflectance spectroscopy and TEM study with applications to Mars SO CLAY MINERALS LA English DT Article DE antigorite; physical alteration; spectroscopy; Mossbauer; reflectance; VNIR; HRTEM; SEM; Mars ID MAGNETITE; MINERALS; SUBSTITUTION; SERPENTINES; KAOLINITE; LIZARDITE; MAGHEMITE; HEMATITE; SPECTRA AB Physical alteration of magnetite-bearing antigorite grains is investigated in this study using Mossbauer, visible/near-infrared (VNIR) and mid-IR spectroscopy coupled with scanning electron microscopy (SEM) and high-resolution transmission electron microscopy (HRTEM) analyses. An expected decrease in grain size with grinding is observed using SEM. The HRTEM images illustrate that the nanophase-sized grains which adhere to larger grains have 7 A antigorite patterns. Mossbauer spectroscopy shows the presence of antigorite, magnetite and an amorphous phase. Visible/near infrared spectra exhibit features common in serpentine. These spectra also show an increasing continuum slope with grinding, an effect which is characteristic of thin coatings or tiny grains on surfaces. Mid-IR spectra indicate the formation of fine-grained Si-OH and carbonate in these samples with grinding. C1 [Bishop, J. L.] NASA, Ames Res Ctr, SETI Inst, Mountain View, CA 94043 USA. [Dyar, M. D.; Sklute, E. C.] Mt Holyoke Coll, S Hadley, MA 01075 USA. [Drief, A.] Clorox Serv Co, Pleasanton, CA 94588 USA. RP Bishop, JL (reprint author), NASA, Ames Res Ctr, SETI Inst, 515 N Whisman Rd, Mountain View, CA 94043 USA. EM Janice.L.Bishop@nasa.gov NR 37 TC 7 Z9 7 U1 1 U2 15 PU MINERALOGICAL SOC PI TWICKENHAM PA 12 BAYLIS MEWS, AMYAND PARK ROAD,, TWICKENHAM TW1 3HQ, MIDDLESEX, ENGLAND SN 0009-8558 EI 1471-8030 J9 CLAY MINER JI Clay Min. PD MAR PY 2008 VL 43 IS 1 BP 55 EP 67 DI 10.1180/claymin.2008.043.1.04 PG 13 WC Chemistry, Physical; Geosciences, Multidisciplinary; Mineralogy SC Chemistry; Geology; Mineralogy GA 289GP UT WOS:000255043300004 ER PT J AU Barsi, S Kassemi, M AF Barsi, S. Kassemi, M. TI Numerical and experimental comparisons of the self-pressurization behavior of an LH2 tank in normal gravity SO CRYOGENICS LA English DT Article DE space cryogenics; hydrogen; heat transfer ID CRYOGENIC TANKS; STORAGE AB In optimizing the design of cryogenic storage facilities for future in-orbit or on-surface applications the boil-off and the self-pressurization rates must be accurately predicted for different g-levels and for a variety of heat loads and distributions. In this paper, a two-phase CFD model is presented that describes the self-pressurization behavior of a flightweight partially full LH2 tank in normal gravity. Existing experimental data at different fill levels are used to assess the predictive capability of the model. The model's predictions indicate favorable agreement with the experimentally measured pressure histories. Small deviations are observed for the median fill level cases where it is suggested that a non-uniform heat load may be the source of this discrepancy. (C) 2008 Elsevier Ltd. All rights reserved. C1 [Barsi, S.] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. Natl Ctr Space Explorat Res, Cleveland, OH USA. RP Barsi, S (reprint author), NASA, Glenn Res Ctr, 21000 Brookpk Rd,Mail Stop 110-3, Cleveland, OH 44135 USA. EM Stephen.J.Barsi@nasa.gov NR 29 TC 12 Z9 16 U1 0 U2 9 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 0011-2275 J9 CRYOGENICS JI Cryogenics PD MAR-APR PY 2008 VL 48 IS 3-4 BP 122 EP 129 DI 10.1016/j.cryogenics.2008.01.003 PG 8 WC Thermodynamics; Physics, Applied SC Thermodynamics; Physics GA 317UY UT WOS:000257046900005 ER PT J AU Welch, RB Sampanes, AC AF Welch, Robert. B. Sampanes, Anthony. C. TI Adapting to virtual environments: Visual-motor skill acquisition versus perceptual recalibration SO DISPLAYS LA English DT Article DE virtual environments; adaptation; intersensory conflicts; sensory-motor conflicts ID PRISM ADAPTATION AB Virtual environment (VE) technology exposes users to a variety of intersensory and sensory-motor discordances to which they must adapt for optimal performance. Our research has distinguished two types of adaptation: Visual-inotor skill acquisition and perceptual recalibration. The first involves learning a new way to coordinate hand and eye, while the second is an automatic, restricted process of perceptual learning. We conclude that an understanding of the controlling conditions and defining characteristics of these two adaptive mechanisms allows one to predict which is the more likely to occur with a given VE and how best to train its users. (c) 2007 Elsevier B.V. All rights reserved. C1 [Welch, Robert. B.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Sampanes, Anthony. C.] Univ Calif Santa Cruz, Dept Psychol, Santa Cruz, CA 95064 USA. RP Welch, RB (reprint author), NASA, Ames Res Ctr, Mail Stop 262-2, Moffett Field, CA 94035 USA. EM Robert.B.Welch@nasa.gov; acsampanes@yahoo.com NR 21 TC 3 Z9 3 U1 1 U2 6 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0141-9382 J9 DISPLAYS JI Displays PD MAR PY 2008 VL 29 IS 2 BP 152 EP 158 DI 10.1016/j.displa.2007.09.013 PG 7 WC Computer Science, Hardware & Architecture; Engineering, Electrical & Electronic; Instruments & Instrumentation; Optics SC Computer Science; Engineering; Instruments & Instrumentation; Optics GA 259BB UT WOS:000252913000013 ER PT J AU Cassady, RJ Frisbee, RH Gilland, JH Houts, MG LaPointe, MR Maresse-Reading, CM Oleson, SR Polk, JE Russell, D Sengupta, A AF Cassady, R. Joseph Frisbee, Robert H. Gilland, James H. Houts, Michael G. LaPointe, Michael R. Maresse-Reading, Colleen M. Oleson, Steven R. Polk, James E. Russell, Derrek Sengupta, Anita TI Recent advances in nuclear powered electric propulsion for space exploration SO ENERGY CONVERSION AND MANAGEMENT LA English DT Article DE space propulsion; electric propulsion; electrostatic; electromagnetic; plasma; nuclear ID MAGNETOPLASMADYNAMIC THRUSTER AB Nuclear and radioisotope powered electric thrusters are being developed as primary in space propulsion systems for potential future robotic and piloted space missions. Possible applications for high-power nuclear electric propulsion include orbit raising and maneuvering of large space platforms, lunar and Mars cargo transport, asteroid rendezvous and sample return, and robotic and piloted planetary missions, while lower power radioisotope electric propulsion could significantly enhance or enable some future robotic deep space science missions. This paper provides an overview of recent US high-power electric thruster research programs, describing the operating principles, challenges, and status of each technology. Mission analysis is presented that compares the benefits and performance of each thruster type for high priority NASA missions. The status of space nuclear power systems for high-power electric propulsion is presented. The paper concludes with a discussion of power and thruster development strategies for future radioisotope electric propulsion systems. (c) 2007 Elsevier Ltd. All rights reserved. C1 [Houts, Michael G.; LaPointe, Michael R.] NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA. [Cassady, R. Joseph] Aerojet Corp, Redmond, WA USA. [Frisbee, Robert H.; Maresse-Reading, Colleen M.; Polk, James E.; Sengupta, Anita] Jet Propuls Lab, Pasadena, CA USA. [Gilland, James H.] Ohio Aerosp Inst, Cleveland, OH USA. [Oleson, Steven R.] NASA, Glenn Res Ctr, Cleveland, OH USA. [Russell, Derrek] Northrop Grumman Space Technol, Redondo Beach, CA USA. RP LaPointe, MR (reprint author), NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA. EM michael.r.lapointe@nasa.gov NR 89 TC 6 Z9 8 U1 0 U2 12 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0196-8904 J9 ENERG CONVERS MANAGE JI Energy Conv. Manag. PD MAR PY 2008 VL 49 IS 3 BP 412 EP 435 DI 10.1016/j.enconman.2007.10.015 PG 24 WC Thermodynamics; Energy & Fuels; Mechanics SC Thermodynamics; Energy & Fuels; Mechanics GA 269SP UT WOS:000253670800005 ER PT J AU Silk, EA Golliher, EL Selvam, RP AF Silk, Eric A. Golliher, Eric L. Selvam, R. Paneer TI Spray cooling heat transfer: Technology overview and assessment of future challenges for micro-gravity application SO ENERGY CONVERSION AND MANAGEMENT LA English DT Article DE spray cooling; heat transfer; micro-gravity; technology development ID MULTIPLE-NOZZLE ARRAYS; DROPLET IMPACT; SINGLE-NOZZLE; FLUX CORRELATION; SURFACE; FC-72; FREON-113; MODELS; WATER; FILM AB Advanced on-board flight systems for future NASA space exploration programs consist of components such as laser-diode arrays (LDA's) and multi-chip modules (MCM's). Thermal management of these systems require high heat flux cooling capability (>= 100 W/ cm 2), tight temperature control (approx. +/- 2 degrees C), reliable start-up (on demand) and long term stability. Traditional multiphase thermal control technologies for space flight (e.g., loop heat pipes, capillary pumped loops, etc.) satisfy the temperature control, start-up and stability requirements, but their heat flux removal capabilities are limited. Spray cooling can provide high heat fluxes in excess of 100 W/cm(2) using fluorinerts and over 1000 W/cm(2) with water while allowing tight temperature control at low coolant fluid flow rates. Spray cooling has been flight proven in an open loop configuration through the Space shuttle's flash evaporator system (FES). However, several closed system issues require investigation to further advance the technology to a technology readiness level (TRL) appropriate for closed system space flight application. This paper provides a discussion of the current status of spray cooling technology as well as NASA's goals, current direction, and challenges associated with the implementation and practice of this technology in the micro-gravity environment. Published by Elsevier Ltd. C1 [Silk, Eric A.] NASA, Goddard Space Flight Ctr, Thermal Engn Technol Dev Grp, Greenbelt, MD 20771 USA. [Golliher, Eric L.] NASA, Glenn Res Ctr, Fluid Phys & Transport Branch, Cleveland, OH 44135 USA. [Selvam, R. Paneer] Univ Arkansas, Power Elect Leveling Solut LLC, Fayetteville, AR 72701 USA. [Selvam, R. Paneer] Univ Arkansas, Computat Mech Lab, Fayetteville, AR 72701 USA. RP Silk, EA (reprint author), NASA, Goddard Space Flight Ctr, Thermal Engn Technol Dev Grp, Greenbelt, MD 20771 USA. EM Eric.A.Silk@nasa.gov; rps@uark.edu RI selvam, Rathinam/H-7849-2013 NR 57 TC 45 Z9 55 U1 6 U2 27 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0196-8904 J9 ENERG CONVERS MANAGE JI Energy Conv. Manag. PD MAR PY 2008 VL 49 IS 3 BP 453 EP 468 DI 10.1016/j.enconman.2007.07.046 PG 16 WC Thermodynamics; Energy & Fuels; Mechanics SC Thermodynamics; Energy & Fuels; Mechanics GA 269SP UT WOS:000253670800007 ER PT J AU Dyson, RW Geng, SM Tew, RC Adelino, M AF Dyson, Rodger W. Geng, Steven M. Tew, Roy C. Adelino, Miguel TI TOWARDS FULLY THREE-DIMENSIONAL VIRTUAL STIRLING CONVERTORS FOR MULTI-PHYSICS ANALYSIS AND OPTIMIZATION SO ENGINEERING APPLICATIONS OF COMPUTATIONAL FLUID MECHANICS LA English DT Article DE computational simulation space power AB The desire for fast, low-cost, and reliable Stirling convertor design decisions has motivated the development of a comprehensive in-house Stirling analysis capability. One of the predominant goals of this project is to enhance the Stirling industry's suite of design tools beyond the currently employed one-dimensional analysis to the level of a virtual three-dimensional full fidelity convertor including structural, mechanical, electromagnetic, and thermal dynamics. This virtual Stirling engine/linear alternator coupling can be used to pre-test prototype hardware, examine internal part performance, and investigate design modifications before expensive convertors are fabricated. An approach is presented for incorporating the complete three-dimensional geometry of modern Stirling convertors and coupling this with multi-physics capability to examine the effects of magnetic, pressure, gravity, spring, and inertial forces on startup behavior, material creep, and overall system performance/efficiency/reliability. C1 [Dyson, Rodger W.; Geng, Steven M.; Tew, Roy C.; Adelino, Miguel] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. RP Dyson, RW (reprint author), NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. EM rodger.w.dyson@nasa.gov FU Science Mission Directorate (SMD); Radioisotope Power System (RPS) Program FX We would like to thank Dr. Kumud Ajmani, Dr. Jim Heldman, Dr. Vijay Garg (late), and Dr. Isaac Lopez for their suggestions and guidance concerning high performance computing and simulation. The work described in this paper was performed for the Science Mission Directorate (SMD) and the Radioisotope Power System (RPS) Program, which provided funding for this project. Any opinions, findings, and conclusions or recommendations expressed in this report are those of the authors and do not necessarily reflect the views of the National Aeronautics and Space Administration. NR 53 TC 2 Z9 2 U1 1 U2 3 PU HONG KONG POLYTECHNIC UNIV, DEPT CIVIL & STRUCTURAL ENG PI HONG KONG PA HUNG HOM, KOWLOON, HONG KONG, 00000, PEOPLES R CHINA SN 1994-2060 J9 ENG APPL COMP FLUID JI Eng. Appl. Comp. Fluid Mech. PD MAR PY 2008 VL 2 IS 1 BP 95 EP 118 PG 24 WC Engineering, Multidisciplinary; Engineering, Mechanical; Mechanics SC Engineering; Mechanics GA V11JC UT WOS:000207526900009 ER PT J AU Kandula, M Nallasamy, R Schallhorn, P Duncil, L AF Kandula, M. Nallasamy, R. Schallhorn, P. Duncil, L. TI AN APPLICATION OF OVERSET GRIDS TO PAYLOAD/FAIRING THREE-DIMENSIONAL INTERNAL FLOW CFD ANALYSIS SO ENGINEERING APPLICATIONS OF COMPUTATIONAL FLUID MECHANICS LA English DT Article DE chimera overset grids; payload/fairing; turbulence models; Navier-Stokes solutions; internal flow AB The application of overset grids to the computational fluid dynamics analysis of three-dimensional internal flow in the payload/fairing of an expendable launch vehicle is described. In conjunction with the overset grid system, the flowfield in the payload/fairing configuration is obtained with the aid of OVERFLOW Navier-Stokes code. The solution exhibits a highly three-dimensional complex flowfield with swirl, separation, and vortices. Some of the computed flow features are compared with the measured Laser-Doppler Velocimetry (LDV) data on a 1/5th scale model of the payload/fairing configuration. The counter-rotating vortex structures and the location of the saddle point predicted by the CFD analysis are in general agreement with the LDV data. Comparisons of the computed (CFD) velocity profiles on horizontal and vertical lines in the LDV measurement plane in the faring nose region show reasonable agreement with the LDV data. C1 [Kandula, M.; Nallasamy, R.] ASRC, Kennedy Space Ctr, FL 32899 USA. [Schallhorn, P.; Duncil, L.] NASA, Kennedy Space Ctr, FL 32899 USA. RP Kandula, M (reprint author), ASRC, Kennedy Space Ctr, FL 32899 USA. EM Max.Kandula-1@nasa.gov FU Kennedy Space Center FX This work was supported by the Launch Services Program (LSP) at Kennedy Space Center. NR 18 TC 1 Z9 1 U1 0 U2 1 PU HONG KONG POLYTECHNIC UNIV, DEPT CIVIL & STRUCTURAL ENG PI HONG KONG PA HUNG HOM, KOWLOON, HONG KONG, 00000, PEOPLES R CHINA SN 1994-2060 J9 ENG APPL COMP FLUID JI Eng. Appl. Comp. Fluid Mech. PD MAR PY 2008 VL 2 IS 1 BP 119 EP 129 PG 11 WC Engineering, Multidisciplinary; Engineering, Mechanical; Mechanics SC Engineering; Mechanics GA V11JC UT WOS:000207526900010 ER PT J AU Liao, K Walker, MF Joshi, A Reschke, M Leigh, RJ AF Liao, Ke Walker, Mark F. Joshi, Anand Reschke, Millard Leigh, R. John TI Vestibulo-ocular responses to vertical translation in normal human subjects SO EXPERIMENTAL BRAIN RESEARCH LA English DT Article DE vestibulo-ocular reflex; locomotion; moving platform ID EYE-MOVEMENTS; LISTINGS LAW; FIXATION DISTANCE; OCULAR RESPONSES; VIEWING DISTANCE; PRIMARY POSITION; SQUIRREL-MONKEY; TARGET DISTANCE; LINEAR MOTION; HEAD AB Prior studies of the human translational vestibulo-ocular reflex (tVOR) report that eye rotations amount to less than 60% of those required to keep the eyes pointed at a stationary visual target, unlike the angular VOR (aVOR) which is optimized to maintain stable gaze. Our first goal was to determine if the performance of the tVOR improves when head translations are combined with head rotations in ambient lighting. A second goal was to measure tVOR during vertical head translations (bob), which has not received systematic study. We measured tVOR alone and in combination with the aVOR in 20 normal human subjects, aged 25-72 years, as they sat on a moving platform that bobbed at 2.0 Hz while rotating horizontally (yaw) at 1.0 Hz. When subjects viewed a visual target at 2 m, median "compensation gain" (eye rotational velocity/required eye rotational velocity to maintain foveal target fixation) was 0.52 during pure bob and 0.59 during combined bob-yaw; during viewing of a near target at similar to 17 cm, compensation gain was 0.58 for pure bob and 0.60 for combined bob-yaw. Mean phase lag of eye-in-head velocity for the tVOR was similar to 19 degrees with respect to the ideal compensatory response, irrespective of whether translation was accompanied by rotation. Thus, the tVOR changed only slightly during translation-rotation versus pure translation, and our subjects' ocular rotations remained at about 60% of those required to point the eyes at the target. Comparison of response during binocular or monocular viewing, and ambient or reduced illumination, indicated that relative image motion between the target and background was an important determinant of tVOR behavior. We postulate that tVOR evolved not to stabilize the image of the target on the fovea, but rather to minimize retinal image motion between objects lying in different planes, in order to optimize motion parallax information. C1 [Walker, Mark F.; Leigh, R. John] Case Western Reserve Univ, Vet Affairs Med Ctr, Dept Neurol, Cleveland, OH 44106 USA. [Liao, Ke; Walker, Mark F.; Joshi, Anand; Leigh, R. John] Case Western Reserve Univ, Univ Hosp, Cleveland, OH 44106 USA. [Liao, Ke; Joshi, Anand; Leigh, R. John] Case Western Reserve Univ, Vet Affairs Med Ctr, Dept Biomed Engn, Cleveland, OH 44106 USA. [Reschke, Millard] Johnson Space Ctr, Neurosci Labs, Houston, TX USA. RP Leigh, RJ (reprint author), Case Western Reserve Univ, Vet Affairs Med Ctr, Dept Neurol, 11100 Euclid Ave, Cleveland, OH 44106 USA. EM rjl4@case.edu RI liao, ke/B-1453-2010 FU NEI NIH HHS [EY06717, R01 EY006717, R01 EY006717-23] NR 38 TC 26 Z9 26 U1 0 U2 6 PU SPRINGER PI NEW YORK PA 233 SPRING STREET, NEW YORK, NY 10013 USA SN 0014-4819 J9 EXP BRAIN RES JI Exp. Brain Res. PD MAR PY 2008 VL 185 IS 4 BP 553 EP 562 DI 10.1007/s00221-007-1181-z PG 10 WC Neurosciences SC Neurosciences & Neurology GA 265LG UT WOS:000253359800003 PM 17989972 ER PT J AU Encinas, JM Vazquez, ME Switzer, RC Chamberland, DW Nick, H Levine, HG Scarpa, PJ Enikolopov, G Steindler, DA AF Encinas, Juan M. Vazquez, Marcelo E. Switzer, Robert C. Chamberland, Dennis W. Nick, Harry Levine, Howard G. Scarpa, Philip J. Enikolopov, Grigori Steindler, Dennis A. TI Quiescent adult neural stem cells are exceptionally sensitive to cosmic radiation SO EXPERIMENTAL NEUROLOGY LA English DT Article ID CENTRAL-NERVOUS-SYSTEM; HIPPOCAMPAL NEUROGENESIS; CONFOCAL MICROSCOPY; IRRADIATION; BRAIN; STEREOLOGY; MARKERS; VITRO AB Generation of new neurons in the adult brain, a process that is likely to be essential for learning, memory, and mood regulation, is impaired by radiation. Therefore, radiation exposure might have not only such previously expected consequences as increased probability of developing cancer, but might also impair cognitive function and emotional stability. Radiation exposure is encountered in settings ranging from cancer therapy to space travel; evaluating the neurogenic risks of radiation requires identifying the at-risk populations of stem and progenitor cells in the adult brain. Here we have used a novel reporter mouse line to find that early neural progenitors are selectively affected by conditions simulating the space radiation environment. This is reflected both in a decrease in the number of these progenitors in the neurogenic regions and in an increase in the number of dying cells in these regions. Unexpectedly, we found that quiescent neural stem cells, rather than their rapidly dividing progeny, are most sensitive to radiation. Since these stem cells are responsible for adult neurogenesis, their death would have a profound impact on the production of new neurons in the irradiated adult brain. Our finding raises an important concern about cognitive and emotional risks associated with radiation exposure. (C) 2007 Elsevier Inc. All rights reserved. C1 [Encinas, Juan M.; Enikolopov, Grigori] Cold Spring Harbor Lab, Cold Spring Harbor, NY 11724 USA. [Vazquez, Marcelo E.] Brookhaven Natl Lab, Upton, NY 11973 USA. [Chamberland, Dennis W.; Levine, Howard G.; Scarpa, Philip J.] NASA, Kennedy Space Ctr, FL USA. [Nick, Harry; Steindler, Dennis A.] Univ Florida, McKnight Brain Inst, Gainesville, FL 32611 USA. RP Enikolopov, G (reprint author), Cold Spring Harbor Lab, 1 Bungtown Rd, Cold Spring Harbor, NY 11724 USA. EM enik@cshl.edu RI Enikolopov, Grigori/B-7771-2009; Encinas, Juan/E-3625-2010; OI Enikolopov, Grigori/0000-0001-8178-8917; Encinas, Juan Manuel/0000-0002-0402-972X FU NHLBI NIH HHS [HL 70143]; NIMH NIH HHS [R21 MH081258, R21 MH081258-01]; NINDS NIH HHS [R01 NS037556, NS 37556] NR 24 TC 20 Z9 21 U1 0 U2 3 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0014-4886 J9 EXP NEUROL JI Exp. Neurol. PD MAR PY 2008 VL 210 IS 1 BP 274 EP 279 DI 10.1016/j.expneurol.2007.10.021 PG 6 WC Neurosciences SC Neurosciences & Neurology GA 270WV UT WOS:000253751800029 PM 18076878 ER PT J AU Grant, JA Irwin, RP Grotzinger, JP Milliken, RE Tornabene, LL McEwen, AS Weitz, CM Squyres, SW Glotch, TD Thomson, BJ AF Grant, John A. Irwin, Rossman P., III Grotzinger, John P. Milliken, Ralph E. Tornabene, Livio L. McEwen, Alfred S. Weitz, Catherine M. Squyres, Steven W. Glotch, Timothy D. Thomson, Brad J. TI HiRISE imaging of impact megabreccia and sub-meter aqueous strata in Holden Crater, Mars SO GEOLOGY LA English DT Article DE Mars; stratigraphy; aqueous; megabreccia ID EVOLUTION AB High Resolution Imaging Science Experiment (HiRISE) images of Holden crater, Mars, resolve impact megabreccia unconformably overlain by sediments deposited during two Noachian-age phases of aqueous activity. A lighter-toned lower unit exhibiting phyllosilicates was deposited in a long-lived, quiescent distal alluvial or lacustrine setting. An overlying darker-toned and often blocky upper unit drapes the sequence and was emplaced during later high-magnitude flooding as an impounded Uzboi Vallis lake overtopped the crater rim. The stratigraphy provides the first geologic context for phyllosilicate deposition during persistent wet and perhaps habitable conditions on early Mars. C1 [Grant, John A.; Irwin, Rossman P., III] Smithsonian Inst, Natl Air & Space Museum, Ctr Earth & Planetary Studies, Washington, DC 20560 USA. [Grotzinger, John P.; Milliken, Ralph E.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. [Tornabene, Livio L.; McEwen, Alfred S.] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA. [Weitz, Catherine M.] Planetary Sci Inst, Tucson, AZ 85719 USA. [Squyres, Steven W.] Cornell Univ, Dept Astron, Ithaca, NY 14853 USA. [Glotch, Timothy D.; Thomson, Brad J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Grant, JA (reprint author), Smithsonian Inst, Natl Air & Space Museum, Ctr Earth & Planetary Studies, Washington, DC 20560 USA. RI Glotch, Timothy/B-6829-2008; OI Thomson, Bradley/0000-0001-8635-8932 NR 21 TC 71 Z9 71 U1 0 U2 7 PU GEOLOGICAL SOC AMER, INC PI BOULDER PA PO BOX 9140, BOULDER, CO 80301-9140 USA SN 0091-7613 EI 1943-2682 J9 GEOLOGY JI Geology PD MAR PY 2008 VL 36 IS 3 BP 195 EP 198 DI 10.1130/G24340A.1 PG 4 WC Geology SC Geology GA 270WN UT WOS:000253751000001 ER PT J AU Pumphrey, HC Boone, C Walker, KA Bernath, P Livesey, NJ AF Pumphrey, H. C. Boone, C. Walker, K. A. Bernath, P. Livesey, N. J. TI Tropical tape recorder observed in HCN SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID ATMOSPHERIC CHEMISTRY; HYDROGEN-CYANIDE; MLS AB The tropical tape recorder is an effect in which a seasonal cycle in the mixing ratio of a gas is imposed on air entering the stratosphere and is then transported upwards by the Brewer-Dobson circulation. We report the observation of this effect in the mixing ratio of HCN, as measured by two satellite instruments: MLS on Aura and ACE-FTS on SCISAT-1. The cycle does not repeat every year; the data so far suggest that the dominant period is about two years. The reason for this periodicity is not yet fully understood. Comparisons with MODIS fire-count data suggest that it may be connected to inter-annual variations in biomass burning in Indonesia and the surrounding region. C1 [Pumphrey, H. C.] Univ Edinburgh, Sch Geosci, Edinburgh, Midlothian, Scotland. [Boone, C.; Walker, K. A.; Bernath, P.] Univ Waterloo, Dept Chem, Waterloo, ON N2L 3G1, Canada. [Livesey, N. J.] NASA, Jet Propuls Lab, Pasadena, CA USA. RP Pumphrey, HC (reprint author), Univ Edinburgh, Sch Geosci, Edinburgh, Midlothian, Scotland. EM pfb500@york.ac.uk RI Bernath, Peter/B-6567-2012 OI Bernath, Peter/0000-0002-1255-396X NR 18 TC 21 Z9 21 U1 1 U2 4 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 EI 1944-8007 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD MAR 1 PY 2008 VL 35 IS 5 AR L05801 DI 10.1029/2007GL032137 PG 6 WC Geosciences, Multidisciplinary SC Geology GA 270IW UT WOS:000253715500002 ER PT J AU Xie, H Gopalswamy, N Cyr, OCS Yashiro, S AF Xie, H. Gopalswamy, N. Cyr, O. C. St. Yashiro, S. TI Effects of solar wind dynamic pressure and preconditioning on large geomagnetic storms SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID TRANSPOLAR POTENTIAL SATURATION; ART. NO. 1341; RING CURRENT; ENERGY-TRANSFER; RAM PRESSURE; DST; INJECTION; DECAY; MODEL AB We investigate the effects of solar wind dynamic pressure, P(dyn), and preconditioning in 88 large magnetic storms (Dst < -100 nT) occurring during solar cycle 23. We have developed an improved model of the Dst profile, based on a modified Burton equation, where additional effects of Pdyn and diminished Dst pressure-correction have been taking into account. On the average, our model predicts the Dst peak values within 9% of observations and gives an overall RMS error of 11%, which is an improvement over those models whose injection functions only depend on the solar wind electric field. The results demonstrate that there is an increase in the Dst peak value when there is a large enhancement of Pdyn during the main phase of a storm. The average increase of the storm intensity is estimated to be 26% for 15 storms with the max (P(dyn)) > 15 nPa. We find that the preconditioning in multi-step Dst storms plays no significant role in strengthening the storm intensity, but increases the storm duration. C1 [Xie, H.; Yashiro, S.] Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA. [Gopalswamy, N.; Cyr, O. C. St.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Xie, H (reprint author), Catholic Univ Amer, Dept Phys, 200 Hannan Hall, Washington, DC 20064 USA. EM hong.xie@ssedmail.gsfc.nasa.gov RI Gopalswamy, Nat/D-3659-2012; OI Gopalswamy, Nat/0000-0001-5894-9954 NR 21 TC 12 Z9 13 U1 0 U2 1 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD MAR 1 PY 2008 VL 35 IS 6 AR L06S08 DI 10.1029/2007GL032298 PG 5 WC Geosciences, Multidisciplinary SC Geology GA 270IX UT WOS:000253715600001 ER PT J AU Chaloupka, M Bjorndal, KA Balazs, GH Bolten, AB Ehrhart, LM Limpus, CJ Suganuma, H Troeeng, S Yamaguchi, M AF Chaloupka, Milani Bjorndal, Karen A. Balazs, George H. Bolten, Alan B. Ehrhart, Llewellyn M. Limpus, Colin J. Suganuma, Hiroyuki Troeeng, Sebastian Yamaguchi, Manami TI Encouraging outlook for recovery of a once severely exploited marine megaherbivore SO GLOBAL ECOLOGY AND BIOGEOGRAPHY LA English DT Article DE Chelonia mydas; conservation; green sea turtle; marine; stock recovery ID TURTLES CHELONIA-MYDAS; SOMATIC GROWTH DYNAMICS; GREEN TURTLE; SEA-TURTLES; COSTA-RICA; SURVIVAL PROBABILITY; POPULATION; DECLINE; TRENDS; CONSERVATION AB Aim To critically review the status of the green sea turtle (Chelonia mydas) using the best available scientific studies as there is a prevailing view that this species is globally endangered and its marine ecosystem functions compromised. Location Ogasawara (Japan), Hawaii (USA), Great Barrier Reef (Australia), Florida (USA), Tortuguero (Costa Rica). Methods We compiled seasonal nesting activity data from all reliable continuous long-term studies (> 25 years), which comprised data series for six of the world's major green turtle rookeries. We estimated the underlying time-specific trend in these six rookery-specific nester or nest abundance series using a generalized smoothing spline regression approach. Results Estimated rates of nesting population increase ranged from c. 4-14% per annum over the past two to three decades. These rates varied considerably among the rookeries, reflecting the level of historical exploitation. Similar increases in nesting population were also evident for many other green turtle stocks that have been monitored for shorter durations than the long-term studies presented here. Main conclusions We show that six of the major green turtle nesting populations in the world have been increasing over the past two to three decades following protection from human hazards such as exploitation of eggs and turtles. This population recovery or rebound capacity is encouraging and suggests that the green turtle is not on the brink of global extinction even though some stocks have been seriously depleted and are still below historical abundance levels. This demonstrates that relatively simple conservation strategies can have a profound effect on the recovery of once-depleted green turtle stocks and presumably the restoration of their ecological function as major marine consumers. C1 [Chaloupka, Milani] Univ Queensland, Ecol Modelling Serv Pty Ltd, St Lucia, Qld 4067, Australia. [Bjorndal, Karen A.; Bolten, Alan B.] Univ Florida, Ctr Sea Turtle Res, Dept Zool, Gainesville, FL 32611 USA. [Balazs, George H.] Pacific Isl Fisheries Sci Ctr, Natl Marine Fisheries Serv, Honolulu, HI 96822 USA. [Ehrhart, Llewellyn M.] Univ Cent Florida, Dept Biol, Orlando, FL 32816 USA. [Ehrhart, Llewellyn M.] Hubbs Sea World Res Inst, Melbourne, FL 32951 USA. [Limpus, Colin J.] Environm Protect Agcy, Queensland Pk & Wildlife Serv, City E, Qld 4002, Australia. [Suganuma, Hiroyuki] Everlasting Nat Asia, Kanagawa Ku, Yokohama, Kanagawa 2210822, Japan. [Troeeng, Sebastian] Carribbean Conservat Corp, San Pedro, Costa Rica. [Troeeng, Sebastian] Lund Univ, Dept Anim Ecol, S-22362 Lund, Sweden. [Yamaguchi, Manami] Ogasawara Marine Ctr, Ogasawara, Tokyo 1002101, Japan. RP Chaloupka, M (reprint author), Univ Queensland, Ecol Modelling Serv Pty Ltd, PO Box 6150, St Lucia, Qld 4067, Australia. EM m.chaloupka@uq.edu.au OI Bjorndal, Karen/0000-0002-6286-1901 NR 61 TC 86 Z9 91 U1 5 U2 35 PU BLACKWELL PUBLISHING PI OXFORD PA 9600 GARSINGTON RD, OXFORD OX4 2DQ, OXON, ENGLAND SN 1466-822X J9 GLOBAL ECOL BIOGEOGR JI Glob. Ecol. Biogeogr. PD MAR PY 2008 VL 17 IS 2 BP 297 EP 304 DI 10.1111/j.1466-8238.2007.00367.x PG 8 WC Ecology; Geography, Physical SC Environmental Sciences & Ecology; Physical Geography GA 259UI UT WOS:000252966000015 ER PT J AU Hood, ED Major, DW Quinn, JW Yoon, WS Gavaskar, A Edwards, EA AF Hood, E. D. Major, D. W. Quinn, J. W. Yoon, W. -S. Gavaskar, A. Edwards, E. A. TI Demonstration of enhanced bioremediation in a TCE source area at Launch Complex 34, Cape Canaveral Air Force Station SO GROUND WATER MONITORING AND REMEDIATION LA English DT Article ID DEHALOCOCCOIDES SP STRAIN; VINYL-CHLORIDE REDUCTASE; CHLOROETHENE BIODEGRADATION; TETRACHLOROETHENE DNAPL; METHANOGENIC CONDITIONS; FIELD DEMONSTRATION; CIS-DICHLOROETHENE; DECHLORINATION; ETHENE; TRICHLOROETHENE AB The ability of bioremediation to treat a source area containing trichloroethene (TCE) present as dense nonaqueous phase liquid (DNAPL) was assessed through a laboratory study and a pilot test at Launch Complex 34, Cape Canaveral Air Force Center. The results of microcosm testing indicate that the indigenous microbial community was capable of dechlorinating TCE to ethene if amended with electron donor; however, bioaugmentation with a dechlorinating culture (KB-1; SiREM, Guelph, Ontario, Canada) significantly increased the rate of ethene formation. In microcosms, the activity of the dechlorinating organisms in KB-1 was not inhibited at initial TCE concentrations as high as 2 mM. The initially high TCE concentration in ground water (1.2 mM or 155 mg/L) did not inhibit reductive dechlorination, and at the end of the study, the average concentration of ethene (2.4 mM or 67 mg/L) was in stoichiometric excess of this initial TCE concentration. The production of ethene in stoichiometric excess in comparison to the initial TCE concentration indicates that the bioremediation treatment enhanced the removal of TCE mass (either sorbed to soil or present as DNAPL). Detailed soil sampling indicated that the bioremediation treatment removed greater than 98.5% of the initial TCE mass. Confirmatory ground water samples collected 22 months after the bioremediation treatment indicated that chloroethene concentrations had continued to decline in the absence of further electron donor addition. The results of this study confirm that dechlorination to ethene can proceed at the high TCE concentrations often encountered in source areas and that bioremediation was capable of removing significant TCE mass from the test plot, suggesting that enhanced bioremediation is a potentially viable remediation technology for TCE source areas. Dehalococcoides abundance increased by 2 orders of magnitude following biostimulation and bioaugmentation. C1 [Hood, E. D.; Major, D. W.] Geosyntec Consultants Inc, Guelph, ON N1G 5G3, Canada. [Quinn, J. W.] NASA, Kennedy Space Ctr, FL 32899 USA. [Yoon, W. -S.; Gavaskar, A.] Battelle Mem Inst, Environm Restorat Sect, Columbus, OH 43201 USA. [Edwards, E. A.] Univ Toronto, Dept Chem Engn & Appl Chem, Toronto, ON M5S 3E5, Canada. RP Hood, ED (reprint author), Geosyntec Consultants Inc, 130 Res Lane,Suite 2, Guelph, ON N1G 5G3, Canada. EM ehood@geosyntec.com OI Edwards, Elizabeth/0000-0002-8071-338X NR 37 TC 22 Z9 27 U1 3 U2 20 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 1069-3629 J9 GROUND WATER MONIT R JI Ground Water Monit. Remediat. PD SPR PY 2008 VL 28 IS 2 BP 98 EP 107 DI 10.1111/j.1745-6592.2008.00197.x PG 10 WC Water Resources SC Water Resources GA 304OO UT WOS:000256119000008 ER PT J AU Lobascio, C Briccarello, M Destefanis, R Faraud, M Gialanella, G Grossi, G Guarnieri, V Manti, L Pugliese, M Rusek, A Scampoli, P Durante, M AF Lobascio, C. Briccarello, M. Destefanis, R. Faraud, M. Gialanella, G. Grossi, G. Guarnieri, V. Manti, L. Pugliese, M. Rusek, A. Scampoli, P. Durante, M. TI Accelerator-based tests of radiation shielding properties of materials used in human space infrastructures SO HEALTH PHYSICS LA English DT Article DE accelerators; carcinogenesis; chromosomal aberration; shielding ID GALACTIC COSMIC-RAYS; EXPOSURE; EXPLORATION; PROTECTION; METAPHASE; MISSIONS; STATION; FE-56 AB Shielding is the only practical countermeasure for the exposure to cosmic radiation during space travel. It is well known that light, hydrogenated materials, such as water and polyethylene, provide the best shielding against space radiation. Kevlar and Nextel are two materials of great interest for spacecraft shielding because of their known ability to protect human space infrastructures from meteoroids and debris. We measured the response to simulated heavy-ion cosmic radiation of these shielding materials and compared it to polyethylene, Lucite (PMMA), and aluminum. As proxy to galactic nuclei we used 1 GeV n(-1) iron or titanium ions. Both physics and biology tests were performed. The results show that Kevlar, which is rich in carbon atoms (about 50% in number), is an excellent space radiation shielding material. Physics tests show that its effectiveness is close (80-90%) to that of polyethylene, and biology data suggest that it can reduce the chromosomal damage more efficiently than PMMA. Nextel is less efficient as a radiation shield, and the expected reduction on dose is roughly half that provided by the same mass of polyethylene. Both Kevlar and Nextel are more effective than aluminum in the attenuation of heavy-ion dose. C1 [Gialanella, G.; Grossi, G.; Manti, L.; Pugliese, M.; Scampoli, P.; Durante, M.] Univ Federico II, Dept Phys & INFN, I-80126 Naples, Italy. [Rusek, A.] Brookhaven Natl Lab, NASA, Space Radiat Lab, Upton, NY 11973 USA. RP Durante, M (reprint author), Univ Federico II, Dipartimento Sci Fis, Via Cintia, I-80126 Naples, Italy. EM Marco.Durante@na.infn.it RI Durante, Marco/K-1315-2014; OI Durante, Marco/0000-0002-4615-553X NR 28 TC 18 Z9 18 U1 1 U2 11 PU LIPPINCOTT WILLIAMS & WILKINS PI PHILADELPHIA PA 530 WALNUT ST, PHILADELPHIA, PA 19106-3621 USA SN 0017-9078 EI 1538-5159 J9 HEALTH PHYS JI Health Phys. PD MAR PY 2008 VL 94 IS 3 BP 242 EP 247 PG 6 WC Environmental Sciences; Public, Environmental & Occupational Health; Nuclear Science & Technology; Radiology, Nuclear Medicine & Medical Imaging SC Environmental Sciences & Ecology; Public, Environmental & Occupational Health; Nuclear Science & Technology; Radiology, Nuclear Medicine & Medical Imaging GA 263XN UT WOS:000253249900003 PM 18301097 ER PT J AU Kraal, ER Asphaug, E Moore, JM Howard, A Bredt, A AF Kraal, Erin R. Asphaug, Erik Moore, Jeffery M. Howard, Alan Bredt, Adam TI Catalogue of large alluvial fans in martian impact craters SO ICARUS LA English DT Article DE Mars; surface; geological processes; Mars; climate ID SEDIMENTARY PROCESSES; LASER ALTIMETER; MARS; LAKES; SYSTEM; FLOW AB We conducted a systematic, global survey using Thermal Emission Imaging System Infrared (THEMIS IR) coverage (similar to 100 m/pixel) to search for large alluvial fans in impact craters on Mars. Our survey has focused on large fans (apron areas greater than similar to 40 km(2), usually located in craters greater than 20 km in diameter) due to the resolution of the THEMIS images and Mars Orbiter Laser Altimeter (MOLA) coverage. We find that the host craters are found to have a distinctive diameter range from 30-150 km. The fans generally cluster in three geographic areas - southern Margaritifer Terra, southwestern Terra Sabaea, and southwestern Tyrrhena Terra, however several outliers do exist. The alluvial fans do not form in a particular orientation along the crater rim nor are they associated with the location of current high rim topography. Fan area magnitude and variability increase with crater diameter while fan concavity magnitude and variability increase with decreasing crater diameter. Smaller fan aprons in general have higher, more variable concavity. The source of the water forming these fans is uncertain given the challenges of accommodating the global distribution pattern and formation patterns within the craters. (C) 2007 Elsevier Inc. All rights reserved. C1 [Kraal, Erin R.; Asphaug, Erik; Bredt, Adam] Univ Calif Santa Cruz, Dept Earth & Planetary Sci, Santa Cruz, CA 95064 USA. [Moore, Jeffery M.] NASA, Ames Res Ctr, Div Space Sci, Moffett Field, CA 94035 USA. [Howard, Alan] Univ Virginia, Dept Environm Sci, Charlottesville, VA 22903 USA. [Kraal, Erin R.] Virginia Tech, Dept Geosci, Blacksburg, VA 24060 USA. RP Kraal, ER (reprint author), Univ Calif Santa Cruz, Dept Earth & Planetary Sci, 1156 High St, Santa Cruz, CA 95064 USA. EM ekraal@vt.edu OI Howard, Alan/0000-0002-5423-1600 NR 29 TC 23 Z9 23 U1 2 U2 10 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 J9 ICARUS JI Icarus PD MAR PY 2008 VL 194 IS 1 BP 101 EP 110 DI 10.1016/j.icarus.2007.09.028 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 267JD UT WOS:000253504400010 ER PT J AU Kitazato, K Clark, BE Abe, M Abe, S Takagi, Y Hiroi, T Arnouin-Jha, OSB Abell, PA Lederer, SM Vilas, F AF Kitazato, Kohei Clark, Beth E. Abe, Masanao Abe, Shinsuke Takagi, Yasuhiko Hiroi, Takahiro Arnouin-Jha, Olivier S. B. Abell, Paul A. Lederer, Susan M. Vilas, Faith TI Near-infrared spectrophotometry of Asteroid 25143 Itokawa from NIRS on the Hayabusa spacecraft SO ICARUS LA English DT Article DE Asteroid Itokawa; photometry; spectrophotometry ID BIDIRECTIONAL REFLECTANCE SPECTROSCOPY; COHERENT BACKSCATTER; GALILEO PHOTOMETRY; OPTICAL-CONSTANTS; SCATTERING; ROUGHNESS; PARTICLES; 433-EROS; LIGHT; MOON AB A photometric analysis of the S-type Asteroid 25143 Itokawa is performed over multiple wavelengths ranging from 0.85 to 2.10 Pm based on disk-resolved reflectance spectra obtained with the Hayabusa near-infrared spectrometer (NIRS). We derive the global photometric properties of Itokawa in terms of Hapke's photometric model. We find that Itokawa has a single-scatter albedo that is 35-40% less than that of Asteroid 433 Eros. Itokawa also has a single-particle phase function that is more strongly back-scattering than that of Eros. Despite its hummocky surface strewn with large boulders, Itokawa exhibits an opposition effect. However, the total amplitude of the opposition surge for Itokawa was estimated to be less than unity while Eros and other S-type asteroids have been found to have model values exceeding unity. The wavelength dependence of the opposition surge width reveals that coherent backscatter contributes to the opposition effect on Itokawa's surface. The photometric roughness of Itokawa is well constrained to a value of 26 degrees +/- 1 degrees which is similar to Eros, suggesting that photometric roughness models the smallest surface roughness scale for which shadows exist. (C) 2007 Elsevier Inc. All rights reserved. C1 [Kitazato, Kohei; Abe, Masanao] Japan Aerosp Explorat Agcy, Inst Space & Astronaut Sci, Sagamihara, Kanagawa 2298510, Japan. [Kitazato, Kohei; Abe, Masanao] Univ Tokyo, Dept Earth & Planetary Sci, Tokyo 1130033, Japan. [Clark, Beth E.] Ithaca Coll, Dept Phys, Ithaca, NY 14850 USA. [Abe, Shinsuke] Kobe Univ, Grad Sch Sci & Technol, Kobe, Hyogo 6518501, Japan. [Takagi, Yasuhiko] Tohoku Gakuin Univ, Nagoya, Aichi 4658515, Japan. [Hiroi, Takahiro] Brown Univ, Dept Geol Sci, Providence, RI 02912 USA. [Arnouin-Jha, Olivier S. B.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA. [Abell, Paul A.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. [Lederer, Susan M.] Calif State Univ San Bernardino, Dept Phys, San Bernardino, CA 92407 USA. [Vilas, Faith] Univ Arizona, MMT Observ, Tucson, AZ 85721 USA. RP Kitazato, K (reprint author), Japan Aerosp Explorat Agcy, Inst Space & Astronaut Sci, 3-1-1 Yoshinodai, Sagamihara, Kanagawa 2298510, Japan. EM kitazato@planeta.sci.isas.jaxa.jp NR 35 TC 18 Z9 18 U1 0 U2 4 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 J9 ICARUS JI Icarus PD MAR PY 2008 VL 194 IS 1 BP 137 EP 145 DI 10.1016/j.icarus.2007.08.029 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 267JD UT WOS:000253504400013 ER PT J AU Gregg, TKP Lopes, RM AF Gregg, Tracy K. P. Lopes, Rosaly M. TI Lava lakes on Io: New perspectives from modeling SO ICARUS LA English DT Article DE Io; Jupiter; satellites; satellites; surfaces; volcanism; geological processes ID EAST PACIFIC RISE; SPREADING MIDOCEAN RIDGES; VOLCANIC-ERUPTIONS; KILAUEA VOLCANO; FLOW-FIELD; HEAT-FLOW; GALILEO; MAGMA; HAWAII; CONSTRAINTS AB Loki Patera (310 degrees W, 12 degrees N) is Io's largest patera at similar to 180 kin in diameter. Its morphology and distinct thermal behavior have led researchers to hypothesize that Loki Patera may either be an active lava lake that experiences periodic overturn, or a shallow depression whose floor is episodically resurfaced with thin flows. Using results from mathematical models, we suggest that a better model for Loki's behavior is the terrestrial superfast spreading East Pacific Rise (EPR), near 17 degrees 30' south. We propose that, like at the southern EPR, Loki Patera is underlain by a thin, persistent magma "lens" that feeds thin, temporary lava lakes within the patera. Also like the southern EPR, overspilling of the volcanic depression is rare. with most of the lava volume being emplaced via a subsurface network of lava tubes. (C) 2007 Elsevier Inc. All rights reserved. C1 [Gregg, Tracy K. P.] SUNY Buffalo, Dept Geol, Buffalo, NY 14260 USA. [Lopes, Rosaly M.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Gregg, TKP (reprint author), SUNY Buffalo, Dept Geol, 876 Nat Sci Complex, Buffalo, NY 14260 USA. EM tgregg@geology.buffalo.edu RI Lopes, Rosaly/D-1608-2016 OI Lopes, Rosaly/0000-0002-7928-3167 NR 55 TC 3 Z9 3 U1 1 U2 5 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 J9 ICARUS JI Icarus PD MAR PY 2008 VL 194 IS 1 BP 166 EP 172 DI 10.1016/j.icarus.2007.08.042 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 267JD UT WOS:000253504400016 ER PT J AU Sekine, Y Imanaka, H Matsui, T Khare, BN Bakes, ELO Mckay, CP Sugita, S AF Sekine, Yasuhito Imanaka, Hiroshi Matsui, Takafumi Khare, Bishun N. Bakes, Emma L. O. Mckay, Christopher P. Sugita, Seiji TI The role of organic haze in Titan's atmospheric chemistry I. Laboratory investigation on heterogeneous reaction of atomic hydrogen with Titan tholin SO ICARUS LA English DT Article DE Titan; organic chemistry; satellites; atmospheres; atmospheres; chemistry ID CARBON-FILMS; METHYL RADICALS; AEROSOLS; ABSTRACTION; SURFACES; PLASMA; GROWTH; MODEL; H-2 AB In Titan's atmosphere consisting of N-2 and CH4, large amounts of atomic hydrogen are produced by photochemical reactions during the formation of complex organics. This atomic hydrogen may undergo heterogeneous reactions with organic aerosol in the stratosphere and mesosphere of Titan. In order to investigate both the mechanisms and kinetics of the heterogeneous reactions, atomic deuterium is irradiated onto Titan tholin formed from N-2 and CH4 gas mixtures at various surface-temperatures of the tholin ranging from 160 to 3 10 K. The combined analyses of the as species and the exposed tholin indicate that the interaction mechanisms of atomic deuterium with the tholin are composed of three reactions; (a) abstraction of hydrogen from tholin resulting in gaseous HD formation (HD recombination), (b) addition of D atom into tholin (hydrogenation), and (c) removal of carbon and/or nitrogen (chemical erosion). The reaction probabilities of HD recombination and hydrogenation are obtained as eta(abst) = 1.9(+/- 0.6) x 10(-3) x exp(-300/T) and eta(hydro) = 2.08(+/- 0.64) x exp(- 1000/T), respectively. The chemical erosion process is very inefficient under the conditions of temperature range of Titan's stratosphere and mesosphere. Under Titan conditions, the rates of hydrogenation > HD recombination >> chemical erosion. Our measured HD recombination rate is about 10 times (with an uncertainty of a factor of 3-5) the prediction of previous theoretical model. These results imply that organic aerosol can remove atomic hydrogen efficiently from Titan's atmosphere through the heterogeneous reactions and that the presence of aerosol may affect the subsequent organic chemistry. (C) 2007 Elsevier Inc. All rights reserved. C1 [Sekine, Yasuhito] Univ Tokyo, Grad Sch Sci, Dept Earth & Planetary Sci, Bunkyo Ku, Tokyo 1130033, Japan. [Imanaka, Hiroshi] Univ Arizona, Dept Chem, Tucson, AZ 85721 USA. [Imanaka, Hiroshi; Khare, Bishun N.; Bakes, Emma L. O.] SETI Inst, Carl Sagan Ctr Study Life Univ, Mountain View, CA 94043 USA. [Matsui, Takafumi; Sugita, Seiji] Univ Tokyo, Grad Sch Frontier Sci, Dept Complex Sci & Engn, Chiba 2278562, Japan. [Khare, Bishun N.; Bakes, Emma L. O.; Mckay, Christopher P.] NASA, Ames Res Ctr, Div Space Sci, Moffett Field, CA 94035 USA. RP Sekine, Y (reprint author), Univ Tokyo, Grad Sch Sci, Dept Earth & Planetary Sci, Bunkyo Ku, 7-3-1 Hongo, Tokyo 1130033, Japan. EM sekine@impact.k.u-tokyo.acjp RI Imanaka, Hiroshi/E-7816-2012 NR 34 TC 37 Z9 37 U1 0 U2 13 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 EI 1090-2643 J9 ICARUS JI Icarus PD MAR PY 2008 VL 194 IS 1 BP 186 EP 200 DI 10.1016/j.icarus.2007.08.031 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 267JD UT WOS:000253504400018 ER PT J AU Sekine, Y Lebonnois, S Imanaka, H Matsui, T Bakes, ELO Mckay, CP Khare, BN Sugita, S AF Sekine, Yasuhito Lebonnois, Sebastien Imanaka, Hiroshi Matsui, Takafumi Bakes, Emma L. O. Mckay, Christopher P. Khare, Bishun N. Sugita, Seiji TI The role of organic haze in Titan's atmospheric chemistry II. Effect of heterogeneous reaction to the hydrogen budget and chemical composition of the atmosphere SO ICARUS LA English DT Article DE Titan; organic chemistry; satellites; atmospheres; atmospheres; chemistry ID POLYCYCLIC AROMATIC-HYDROCARBONS; AEROSOLS; MODEL; PHOTOCHEMISTRY; CONSTITUENTS; SPECTROSCOPY; SENSITIVITY; DIACETYLENE; BENZENE; METHANE AB One of the key components controlling the chemical composition and climatology of Titan's atmosphere is the removal of reactive atomic hydrogen from the atmosphere. A proposed process of the removal of atomic hydrogen is the heterogeneous reaction with organic aerosol. In this study, we investigate the effect of heterogeneous reactions in Titan's atmospheric chemistry using new measurements of the heterogeneous reaction rate [Sekine, Y., Imanaka, H., Matsui, T., Khare, B.N., Bakes, E.L.O., McKay, C.P., Sugita, S., 2008. Icarus 194, 186-200] in a one-dimensional photochemical model. Our results indicate that 60-75% of the atomic hydrogen in the stratosphere and mesosphere are consumed by the heterogeneous reactions. This result implies that the heterogeneous reactions on the aerosol surface may predominantly remove atomic hydrogen in Titan's stratosphere and mesosphere. The results of our calculation also indicate that a low concentration of atomic hydrogen enhances the concentrations of unsaturated complex organics, such as C4H2 and phenyl radical, by more than two orders in magnitude around 400 km in altitude. Such an increase in unsaturated species may induce efficient haze production in Titan's mesosphere and upper stratosphere. These results imply a positive feedback mechanism in haze production in Titan's atmosphere. The increase in haze production would affect the chemical composition of the atmosphere, which might induce further haze production. Such a positive feedback could tend to dampen the loss and supply cycles of CH4 due to an episodic CH4 release into Titan's atmosphere. (C) 2007 Elsevier Inc. All rights reserved. C1 [Sekine, Yasuhito] Univ Tokyo, Grad Sch Sci, Dept Earth & Planetary Sci, Bunkyo Ku, Tokyo 1130033, Japan. UPMC, CNRS, Meteorol Dynam Lab, IPSL, F-75252 Paris, France. [Imanaka, Hiroshi; Bakes, Emma L. O.] Univ Arizona, Dept Chem, Tucson, AZ 85721 USA. [Imanaka, Hiroshi; Khare, Bishun N.] SETI Inst, Mountain View, CA 94043 USA. [Matsui, Takafumi; Sugita, Seiji] Univ Tokyo, Grad Sch Frontier Sci, Dept Complex Sci & Engn, Chiba 2778562, Japan. [Bakes, Emma L. O.; Mckay, Christopher P.; Khare, Bishun N.] NASA, Ames Res Ctr, Div Space Sci, Moffett Field, CA 94035 USA. RP Sekine, Y (reprint author), Univ Tokyo, Grad Sch Sci, Dept Earth & Planetary Sci, Bunkyo Ku, 7-3-1 Hongo, Tokyo 1130033, Japan. EM sekine@impact.k.u-tokyo.ac.jp RI Imanaka, Hiroshi/E-7816-2012 NR 47 TC 23 Z9 23 U1 0 U2 15 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 EI 1090-2643 J9 ICARUS JI Icarus PD MAR PY 2008 VL 194 IS 1 BP 201 EP 211 DI 10.1016/j.icarus.2007.08.030 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 267JD UT WOS:000253504400019 ER PT J AU McCord, TB Hayne, P Combe, JP Hansen, GB Barnes, JW Rodriguez, S Le Mouelic, S Baines, EKH Buratti, BJ Sotin, C Nicholson, P Jaumann, R Nelson, R AF McCord, Thomas B. Hayne, Paul Combe, Jean-Philippe Hansen, Gary B. Barnes, Jason W. Rodriguez, Sebastien Le Mouelic, Stephane Baines, E. Kevin H. Buratti, Bonnie J. Sotin, Christophe Nicholson, Philip Jaumann, Ralf Nelson, Robert CA Cassini VIMS Team TI Titan's surface: Search for spectral diversity and composition using the Cassini VIMS investigation SO ICARUS LA English DT Article DE Saturn; satellites; satellites; surfaces; spectroscopy ID GALILEAN SATELLITES; WATER-ICE; REFLECTANCE; ABSORPTION; MIXTURES; WINDS AB The surface composition of Titan is of great importance for understanding both the internal evolution of Titan and its atmosphere. The Visual and Infrared Mapping Spectrometer (VIMS) investigation on Cassini is observing Titan from 0.35 to 5.11 mu m with spatial resolution down to a few kilometers during each flyby of the spacecraft as it orbits Saturn. Our search for spectral diversity using seven methane transmission windows in the near infrared suggests that spectrally distinct units exist on the surface of Titan and that most of the surface can be modeled using only a few distinct spectral units: water frost, CO2 frost, atmospheric scattering, and an unknown material bright at 2 mu m. A dark, spectrally neutral material is also implied. Use of an atmospheric scattering component with spectral mixing analysis may provide a method for partially removing atmospheric effects. In some locations, atmospheric scattering accounts for the majority of the signal. There are also small regions with unusual spectra that may be due to low signal and high noise and/or may be exotic materials of interest. Further, we searched within the methane windows for spectral features associated with Titan's surface. Only the 5-mu m and, to a lesser extent, the 2-mu m window provide a reasonable opportunity for this as the shorter-wavelength windows are too narrow and the 2.8-mu m window is cluttered with an unknown atmospheric constituent. We find evidence for only one spectral feature: near 4.92 mu m for the 5-mu m bright Tui Regio region. CO2 frost with grains smaller than about 10 Pm is the best candidate we have found so far to explain this absorption as well as the feature's spectral contrast between the 2.7- and the 2.8-mu m atmosphere subwindows. This suggested CO2 identification is supported by the presence of an endmember in the spectral mixture analysis that is consistent with CO2 frost with large grain sizes. We find no other absorption features that are statistically significant, including those reported earlier by others. These results are consistent with but greatly extend our early analysis that treated only the T-a data set [McCord, T.B., et al., 2006a. Planet. Space Sci. 54, 1524-1539]. In the spectral feature search process, we explored in detail the noise characteristics of the VIMS data within the 5-mu m window. which has generally very low signal (4-20 DN), due to the measurement conditions and low illumination levels. We find noise of nearly Gaussian statistics except for some erratic darks and noise spikes, and the data set seems generally well behaved. We present examples of our attempt to improve on the standard VIMS pipeline data calibration. (C) 2007 Elsevier Inc. All rights reserved. C1 [McCord, Thomas B.; Hayne, Paul; Combe, Jean-Philippe; Hansen, Gary B.] Bear Flight Ctr, Winthrop, WA 98862 USA. [Hayne, Paul] Univ Calif Los Angeles, Dept Earth & Space Sci, Los Angeles, CA 90095 USA. [Hansen, Gary B.] Univ Washington, Dept Earth & Space Sci, Seattle, WA 98195 USA. [Barnes, Jason W.] Univ Arizona, Dept Planetary Sci & LPL, Tucson, AZ 85721 USA. [Rodriguez, Sebastien] Ctr Etud Saclay, DAPNIA SAp, F-91191 Gif Sur Yvette, France. [Le Mouelic, Stephane; Sotin, Christophe] Univ Nantes, LPG Nantes, F-44322 Nantes, France. [Baines, E. Kevin H.; Buratti, Bonnie J.; Nelson, Robert] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Nicholson, Philip] Cornell Univ, Dept Astron, Ithaca, NY 14853 USA. [Jaumann, Ralf] DLR, Inst Planetary Res, D-12489 Berlin, Germany. RP McCord, TB (reprint author), Bear Flight Ctr, POB 667,22 Fiddlers Rd, Winthrop, WA 98862 USA. EM mccordtb@aol.com RI Barnes, Jason/B-1284-2009; Rodriguez, Sebastien/H-5902-2016 OI Barnes, Jason/0000-0002-7755-3530; Rodriguez, Sebastien/0000-0003-1219-0641 NR 55 TC 47 Z9 48 U1 0 U2 10 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 J9 ICARUS JI Icarus PD MAR PY 2008 VL 194 IS 1 BP 212 EP 242 DI 10.1016/j.icarus.2007.08.039 PG 31 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 267JD UT WOS:000253504400020 ER PT J AU Achterberg, RK Conrath, BJ Gierasch, PJ Flasar, EM Nixon, CA AF Achterberg, Richard K. Conrath, Barney J. Gierasch, Peter J. Flasar, E. Michael Nixon, Conor A. TI Titan's middle-atmospheric temperatures and dynamics observed by the Cassini Composite Infrared Spectrometer SO ICARUS LA English DT Article DE Titan; atmospheres; structure; atmospheres; dynamics; infrared observations ID LATITUDINAL VARIATIONS; GENERAL-CIRCULATION; STRATOSPHERE; VORTEX; OCCULTATION; PROFILES; EMISSION; SPECTRA; DESCENT; MODEL AB The Composite Infrared Radiometer-Spectrometer (CIRS) instrument, on the NASA Cassini Saturn orbiter, has been acquiring thermal emission spectra from the atmosphere of Titan since orbit insertion in 2004. Observation sequences for measuring stratospheric temperatures have been obtained using both a nadir mapping mode and a limb viewing mode. The limb observations give better vertical resolution, and give information from higher altitudes, while the nadir observations provide more complete longitude coverage. Because the scale height of Titan's atmosphere is large enough so that emission from a grazing ray is influenced by horizontal temperature variations in the atmosphere, we have developed a two-dimensional temperature retrieval algorithm for reducing the limb spectra, which solves simultaneously for meridional and vertical temperature variations. The analyzed nadir mapping data have sampled nearly all longitudes at latitudes from about 90 degrees S to 60 degrees N, providing temperatures between pressure levels of about 5 to 0.2 mbar. The limb data covers latitudes between about 75 degrees S and 85 degrees N, and yields temperatures between about 1 and 0.005 mbar, at a small number of longitudes. The retrieved temperatures are consistent with early results from nadir observations [Flasar, F.M., and 44 colleagues, 2005. Science 308, 975-978] between 0.5 and 5 mbar where both results are valid, with the warmest temperatures at the equator, and much stronger meridional temperature gradients in the northern (winter) hemisphere than in the southern. At higher altitudes not probed by nadir viewing, the limb data reveal that the stratopause is nearly 20 K warmer in the northern polar regions than at the equator and southern hemisphere, and that the altitude of the stratopause shifts from approximate to 0.1 mbar (300 km) near the equator to 0.01 mbar (400 km) poleward of about 40 degrees N. When the gradient wind equation is used to construct a zonal mean wind, the reversal in sign of the temperature leads to capping of the winter westerly flow. The core of the resulting jet is about 190 m s(-1) in magnitude, spans between 30 degrees N and 60 degrees N, and peaks near 0.1 mbar. Estimates of the radiative heating associated with the radiative disequilibrium lead to a meridional overturning timescale of about three Earth years. (C) 2007 Elsevier Inc. All rights reserved. C1 [Achterberg, Richard K.; Nixon, Conor A.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Conrath, Barney J.; Gierasch, Peter J.] Cornell Univ, Dept Astron, Ithaca, NY 14853 USA. [Flasar, E. Michael] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Achterberg, RK (reprint author), Univ Maryland, Dept Astron, College Pk, MD 20742 USA. EM richard.k.achterberg@nasa.gov RI Nixon, Conor/A-8531-2009; Flasar, F Michael/C-8509-2012 OI Nixon, Conor/0000-0001-9540-9121; NR 39 TC 86 Z9 86 U1 0 U2 6 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 J9 ICARUS JI Icarus PD MAR PY 2008 VL 194 IS 1 BP 263 EP 277 DI 10.1016/j.icarus.2007.09.029 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 267JD UT WOS:000253504400022 ER PT J AU Magee-Sauer, K Mumma, MJ DiSanti, MA Dello Russo, N Gibb, EL Bonev, BP Villanueva, GL AF Magee-Sauer, Karen Mumma, Michael J. DiSanti, Michael A. Dello Russo, Neil Gibb, Erika L. Bonev, Boncho P. Villanueva, G. L. TI The organic composition of Comet C/2001 A2 (LINEAR) I. Evidence for an unusual organic chemistry SO ICARUS LA English DT Article DE comets; comets; composition; spectroscopy ID O1 HALE-BOPP; C/1996 B2 HYAKUTAKE; OH PROMPT EMISSION; WATER PRODUCTION; CARBON-MONOXIDE; SPECTROSCOPIC OBSERVATIONS; RADIO TELESCOPES; PARENT VOLATILES; FRAGMENT-C; H1 LEE AB We used the NIRSPEC instrument on the Keck-2 telescope atop Mauna Kea, HI to observe Comet C/2001 A2 (LINEAR) in a Target of Opportunity campaign on UT 2001 July 9.5, 10.5 August 4.4, 10.5. We measured seven organic parent volatiles (C2H6, C2H2, HCN, CH4, CO, CH3OH, H2CO) simultaneously with H2O. We obtained absolute production rates and relative abundances for parent volatiles, and also measured rotational temperatures for several of these species. The chemical composition of C/2001 A2 differs substantially from any comet we have observed to date. The abundances we measure (relative to H2O) for C2H6, C2H2, HCN, and CH3OH are enriched by a factor of similar to 2 to 3 in C/2001 A2 compared with most comets in our database. Other molecular species were detected within the typical range of measured abundances. C/2001 A2 presented a unique opportunity to study the chemistry of a fragmenting comet where pristine areas are exposed to the Sun. (c) 2007 Elsevier Inc. All rights reserved. C1 [Magee-Sauer, Karen] Rowan Univ, Dept Phys & Astron, Glassboro, NJ 08028 USA. [Mumma, Michael J.; DiSanti, Michael A.; Bonev, Boncho P.; Villanueva, G. L.] NASA, Goddard Space Flight Ctr, Solar Syst Explorat Div, Greenbelt, MD 20771 USA. [Dello Russo, Neil] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA. [Gibb, Erika L.] Univ Missouri, Dept Phys & Astron, St Louis, MO 63121 USA. [Bonev, Boncho P.] Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA. RP Magee-Sauer, K (reprint author), Rowan Univ, Dept Phys & Astron, Glassboro, NJ 08028 USA. EM sauer@rowan.edu RI mumma, michael/I-2764-2013; Magee-Sauer, Karen/K-6061-2015; Dello Russo, Neil/G-2727-2015 OI Magee-Sauer, Karen/0000-0002-4979-9875; Dello Russo, Neil/0000-0002-8379-7304 NR 55 TC 35 Z9 35 U1 1 U2 3 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 J9 ICARUS JI Icarus PD MAR PY 2008 VL 194 IS 1 BP 347 EP 356 DI 10.1016/j.icarus.2007.10.006 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 267JD UT WOS:000253504400027 ER PT J AU Cooper, PD Moore, MH Hudson, RL AF Cooper, Paul D. Moore, Marla H. Hudson, Reggie L. TI Radiation chemistry of H2O+O-2 ices SO ICARUS LA English DT Article DE ices; IR spectroscopy; satellites; composition; Europa; Ganymede; enceladus ID ELECTRON-STIMULATED PRODUCTION; CRYSTALLINE WATER ICE; AMORPHOUS SOLID WATER; HYDROGEN-PEROXIDE; INFRARED-SPECTROSCOPY; ION IRRADIATION; GALILEAN SATELLITES; MOLECULAR-OXYGEN; MATRIX-ISOLATION; FAR-IR AB The chemistry and spectroscopy of proton-irradiated H2O + O-2 ices have been investigated in relation to the production of oxidants in icy satellite surfaces. Hydrogen peroxide (H2O2), ozone (O-3), and the hydroperoxy (HO2) and hydrogen trioxide (HO3) radicals have all been observed, and their temperature and dose dependent production trends have been measured. We find that O-2 aggregates form during the growth of H2O + O-2 ice films, and the presence of these aggregates greatly affects the HO2 and H2O2 yields. In addition, we have found that the position of the spectral maximum of the v(3) vibration of O-3 shifts with ice composition, giving an indication of the degree of dispersion of O-3 molecules within the ice. We discuss the relevance of these measurements to icy satellite surfaces. (c) 2007 Elsevier Inc. All rights reserved. C1 [Cooper, Paul D.; Moore, Marla H.] NASA, Goddard Space Flight Ctr, Astrochem Branch, Greenbelt, MD 20771 USA. [Hudson, Reggie L.] Eckerd Coll, Dept Chem, St Petersburg, FL 33711 USA. RP Cooper, PD (reprint author), George Mason Univ, Dept Chem & Biochem, MS 3E2,4400 Univ Dr, Fairfax, VA 22030 USA. EM pcooper6@gmu.edu RI Hudson, Reggie/E-2335-2012 NR 44 TC 25 Z9 25 U1 4 U2 12 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 J9 ICARUS JI Icarus PD MAR PY 2008 VL 194 IS 1 BP 379 EP 388 DI 10.1016/j.icarus.2007.10.002 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 267JD UT WOS:000253504400030 ER PT J AU Zell, E Engel-Cox, J Eckman, R Stackhouse, P AF Zell, Erica Engel-Cox, Jill Eckman, Richard Stackhouse, Paul, Jr. TI Application of Satellite Sensor Data and Models for Energy Management SO IEEE JOURNAL OF SELECTED TOPICS IN APPLIED EARTH OBSERVATIONS AND REMOTE SENSING LA English DT Article AB Effective, environmentally sound development, production, and delivery of energy depend on Earth monitoring information. Satellite remote sensing data and products provide unique, objective information that has the additional advantage of yielding global, homogeneous, and repetitive coverage. Satellite remote sensing data and products have been used extensively in parts of the energy sector for applications ranging from climatology to identification of solar and wind energy sources, vet there is significant potential to expand energy applications. This paper discusses the key energy sector organizations and decision-support tools with the greatest potential to benefit from new applications of satellite remote sensing data, identifies relevant remote sensing data and products with a focus on NASA Earth science resources, and provides examples that show the added value of the Earth observations. These examples come from the application of NASA data to solar energy information needs. Although continued work for support of solar energy is warranted, this paper focuses on areas identified with the greatest demonstrated potential for new or expanded applications: renewable energy (specifically wind, biomass, and hydroelectric resources), load forecasting, and long-term energy modeling. This study also addresses the evolving context of the Global Earth Observation System of Systems (GEOSS), and the broader framework of integrating satellite remote sensing into energy sector decision-support tools. C1 [Zell, Erica; Engel-Cox, Jill] Battelle Mem Inst, Arlington, VA 22201 USA. [Eckman, Richard] US Natl Aeronaut & Space Adm, Langley Res Ctr, Sci Directorate, Chem & Dynam Branch, Hampton, VA 23681 USA. [Stackhouse, Paul, Jr.] US Natl Aeronaut & Space Adm, Langley Res Ctr, Sci Directorate, Climate Sci Branch, Hampton, VA 23681 USA. RP Zell, E (reprint author), Battelle Mem Inst, Arlington, VA 22201 USA. EM zelle@battelle.org FU NASA Earth Science Applied Sciences FX This work was Supported by the NASA Earth Science Applied Sciences program under the Energy Management theme. NR 36 TC 3 Z9 3 U1 1 U2 6 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855 USA SN 1939-1404 J9 IEEE J-STARS JI IEEE J. Sel. Top. Appl. Earth Observ. Remote Sens. PD MAR PY 2008 VL 1 IS 1 BP 5 EP 17 DI 10.1109/JSTARS.2008.2001142 PG 13 WC Engineering, Electrical & Electronic; Geography, Physical; Remote Sensing; Imaging Science & Photographic Technology SC Engineering; Physical Geography; Remote Sensing; Imaging Science & Photographic Technology GA 436MM UT WOS:000265418200003 ER PT J AU Lee, M Wanke, MC Lerttamrab, M Young, EW Grine, AD Reno, JL Siegel, PH Dengler, RJ AF Lee, Mark Wanke, Michael C. Lerttamrab, Maytee Young, Erik W. Grine, Albert D. Reno, John L. Siegel, Peter H. Dengler, Robert J. TI Heterodyne mixing of terahertz quantum cascade lasers using a planar Schottky diode SO IEEE JOURNAL OF SELECTED TOPICS IN QUANTUM ELECTRONICS LA English DT Article DE heterodyne mixing; quantum cascade laser (QCL); Schottky diode; terahertz (THz) AB Terahertz quantum cascade lasers (QCLs) have been used together with a monolithic planar Schottky diode receiver to study the heterodyne mixing between dual internal modes of a QCL and between a single mode of a QCL and a known molecular line from a molecular gas laser. Dual-mode mixing shows that I e intrinsic linewidth of a free-running QCL is <= 30 kHz. Mixing against a molecular laser line gives a high precision measurement of a QCL's absolute frequency and can show transient turn-on behavior in a pulsed QCL. C1 [Lee, Mark; Wanke, Michael C.; Lerttamrab, Maytee; Young, Erik W.; Grine, Albert D.; Reno, John L.] Sandia Natl Labs, Albuquerque, NM 87185 USA. [Siegel, Peter H.; Dengler, Robert J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Lee, M (reprint author), Sandia Natl Labs, POB 5800, Albuquerque, NM 87185 USA. EM mlee1@sandia.gov; mcwanke@sandia.gov; mlertta@sandia.gov; ewyoung@sandia.gov; adgrine@sandia.gov; jlreno@sandia.gov; phs@caltech.edu; no6b@no6b.nasa.gov FU United States Department of Energy's National Nuclear Security Administration [DE-AC04-94AL85000] FX Sandia is a multiprogram laboratory operated by Sandia Corporation, a Lockheed Martin Company, for the United States Department of Energy's National Nuclear Security Administration under Contract DE-AC04-94AL85000. NR 11 TC 17 Z9 17 U1 0 U2 5 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855 USA SN 1077-260X J9 IEEE J SEL TOP QUANT JI IEEE J. Sel. Top. Quantum Electron. PD MAR-APR PY 2008 VL 14 IS 2 BP 370 EP 373 DI 10.1109/JSTQE.2007.910762 PG 4 WC Engineering, Electrical & Electronic; Optics; Physics, Applied SC Engineering; Optics; Physics GA 342CY UT WOS:000258763400014 ER PT J AU Maestrini, A Ward, JS Tripon-Canseliet, C Gill, JJ Lee, C Javadi, H Attopadhyay, GC Mehdi, I AF Maestrini, Alain Ward, John S. Tripon-Canseliet, Charlotte Gill, John J. Lee, Choonsup Javadi, Hamid Attopadhyay, Goutam Ch. Mehdi, Imran TI In-phase power-combined frequency triplers at 300 GHz SO IEEE MICROWAVE AND WIRELESS COMPONENTS LETTERS LA English DT Article DE frequency multiplier; frequency tripler; local oscillator; planar diode; power-combining; Schottky diode; sub-millimeter wavelengths; varactor AB We report on the design, fabrication and characterization of a 300 GHz Schottky-diode frequency tripler made of two mirror-image integrated circuits that are power-combined in-phase in a single waveguide block using compact Y-junctions at the input and output waveguides. Each chip features six anodes on a 5 mu m thick GaAs membrane. The tripler has 5-15% conversion efficiency measured across the 265-330 GHz band when driven with 50-250 mW of input power at room temperature. At 318 GHz it delivers a peak power of 26 mW with 11 % conversion efficiency. The power-combined frequency multiplier is compared with a single-chip tripler designed for the same band using the same integrated circuit. C1 [Maestrini, Alain] Univ Paris 06, LISIF, Paris, France. [Maestrini, Alain] Observ Paris, Lerma, France. [Ward, John S.; Gill, John J.; Javadi, Hamid; Attopadhyay, Goutam Ch.; Mehdi, Imran] CALTECH, Jet Propuls Lab, Pasadena, CA 91125 USA. [Tripon-Canseliet, Charlotte] Univ Paris 06, LISIF, F-75005 Paris, France. RP Maestrini, A (reprint author), Univ Paris 06, LISIF, Paris, France. EM alain.maestrini@obspm.fr; john.ward@jpl.nasa.gov; Charlotte.Canseliet@lisif.jussieu.fr NR 6 TC 31 Z9 33 U1 0 U2 5 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855 USA SN 1531-1309 J9 IEEE MICROW WIREL CO JI IEEE Microw. Wirel. Compon. Lett. PD MAR PY 2008 VL 18 IS 3 BP 218 EP 220 DI 10.1109/LMWC.2008.916820 PG 3 WC Engineering, Electrical & Electronic SC Engineering GA 273FZ UT WOS:000253917100024 ER PT J AU Feather, MS Cornford, SL Hicks, KA Kiper, JD Menzies, T AF Feather, Martin S. Cornford, Steven L. Hicks, Kenneth A. Kiper, James D. Menzies, Tim TI A broad, quantitative model for making early requirements decisions SO IEEE SOFTWARE LA English DT Article C1 [Feather, Martin S.; Cornford, Steven L.] CALTECH, Jet Propuls Lab, Pasadena, CA 91125 USA. [Hicks, Kenneth A.] CALTECH, Jet Propuls Lab, Syst Modeling & Analysis Program Off, Pasadena, CA 91125 USA. [Kiper, James D.] Miami Univ, Sch Engn & Appl Sci, Oxford, OH 45056 USA. [Menzies, Tim] W Virginia Univ, Morgantown, WV 26506 USA. RP Feather, MS (reprint author), CALTECH, Jet Propuls Lab, Pasadena, CA 91125 USA. EM Martin.S.Feather@ipl.nasa.gov; Steven.L.Cornford@ipl.nasa.gov; Kenneth.A.Hicks@ipl.nasa.gov; kiperjd@muohio.edu; tim@menzies.us NR 14 TC 8 Z9 8 U1 0 U2 1 PU IEEE COMPUTER SOC PI LOS ALAMITOS PA 10662 LOS VAQUEROS CIRCLE, PO BOX 3014, LOS ALAMITOS, CA 90720-1314 USA SN 0740-7459 EI 1937-4194 J9 IEEE SOFTWARE JI IEEE Softw. PD MAR-APR PY 2008 VL 25 IS 2 BP 49 EP 56 DI 10.1109/MS.2008.29 PG 8 WC Computer Science, Software Engineering SC Computer Science GA 265QN UT WOS:000253376100019 ER PT J AU Weisbin, CR Smith, JH Van Houten, T Moeller, R Zimmerman, W Smythe, W Lincoln, W Elfes, A Adumitroaie, V Silberg, R AF Weisbin, Charles R. Smith, Jeffrey H. Van Houten, Tracy Moeller, Robert Zimmerman, Wayne Smythe, William Lincoln, William Elfes, Alberto Adumitroaie, Virgil Silberg, Robert TI Technical Feasibility and Relative Productivity of Alternate NASA Robotic Missions to a Lunar Dark Crater SO IEEE SYSTEMS JOURNAL LA English DT Article DE Analysis software; decision making; exploration; fuel cell; NASA lunar missions; optimization; power sources; productivity; return on investment; radioisotope thermoelectric generator (RTG); technology development; value AB Two concepts for large-scale, complex, robotic missions to search for frozen water at the lunar South Pole are systematically analyzed to determine their relative productivity and investment requirements. A concurrent design team, a technology-assessment tool, and a sensitivity model are integrated to search a large, complex trade space. Performance goals for a broad portfolio of missions comprising NASA's lunar exploration program are optimized subject to budget, workforce, and other nontechnical constraints. Explicit distinction is made between enabling and enhancing technologies. Uncertainties and dependencies are included within the optimization framework. Given the constraints used in this analysis, the study determines that the longer mission [using a radioisotope thermoelectric generator (RTG)] would return 14 times the value of the shorter mission (using a methanol-oxygen fuel cell) for roughly a 17% increase in cost, and would be enabled with the recommended temporal technology portfolio. To assess the robustness of the investment recommendations, other potential fuel-cell chemistries are evaluated along with potential improvements in rover speed and autonomy, and a reduced activity profile. Results indicate that a lithium-oxygen fuel cell would enable the highest level of productivity among the three fuel cells studied, though not as high as that permitted by an RTG. For the shorter duration mission concepts, it was found that productivity could be enhanced by reducing the number of activities from the baseline 15 to 4, thereby permitting time for each activity to be more fully accomplished. C1 [Weisbin, Charles R.; Silberg, Robert] CALTECH, Jet Prop Lab, Web Solut Grp, Raytheon, Pasadena, CA 91109 USA. RP Weisbin, CR (reprint author), CALTECH, Jet Prop Lab, Web Solut Grp, Raytheon, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM charles.r.weisbin@jpl.nasa.gov RI Elfes, Alberto/E-2463-2011 OI Elfes, Alberto/0000-0003-2433-995X FU LaRC; Exploration Technology Development Program (ETDP) FX The authors would like to thank J. Falker (currently at the NASA Johnson Space Center); J. Derleth and B. Claybaugh of NASA Program Analysis and Evaluation (PA & E); D. Craig of the Exploration Systems Mission Directorate Integration Office (DIO); P. Troutman of LaRC supporting the DIO; C. Moore of the ESMD Advanced Capabilities Division (ACD); F. Peri and D. Beals of the Exploration Technology Development Program (ETDP) who support ACD; R. Wheeler and M. Adler leading the Team X Concurrent Design Effort; and S. Prusha who manages the System Modeling and Analysis Program Office for graciously contributing resources, analytical review and critique, and advocacy for this effort. They would also like to thank A. Loverro, who helped guide the Team X design session; S. Sherrit, who provided invaluable information about drilling and sample acquisition; K. Shelton, who helped formulate and manipulate the resulting START database; and H. Hua and J. Mrozinski who implemented the START optimization algorithms and associated output display. Finally, the authors would like to thank R. Orozco who converted the substance of this paper into the format required by the publication. NR 14 TC 1 Z9 1 U1 1 U2 8 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 1932-8184 EI 1937-9234 J9 IEEE SYST J JI IEEE Syst. J. PD MAR PY 2008 VL 2 IS 1 BP 120 EP 128 DI 10.1109/JSYST.2007.908171 PG 9 WC Computer Science, Information Systems; Engineering, Electrical & Electronic; Operations Research & Management Science; Telecommunications SC Computer Science; Engineering; Operations Research & Management Science; Telecommunications GA V10NC UT WOS:000207469700013 ER PT J AU Morabito, DD Imbriale, W Keihm, S AF Morabito, David D. Imbriale, William Keihm, Stephen TI Observing the Moon at microwave frequencies using a large-diameter deep space network antenna SO IEEE TRANSACTIONS ON ANTENNAS AND PROPAGATION LA English DT Article DE antenna radiation patterns; microwave antennas; Moon; temperature measurement AB The Moon radiates energy at infrared and microwave wavelengths, in addition to reflecting sunlight at optical wavelengths. As a result, an antenna pointed at or near the Moon will result in an increase in system operating noise temperature, which needs to be accounted for in RF telecommunications, radio science or radiometric link calculations. The NASA Deep Space Network (DSN) may use its large-diameter antennas in future lunar robotic or human missions, and thus it is important to understand the nature of this temperature increase as a function of observing frequency, lunar phase, and angular position of the antenna beam on the lunar disk. This paper reports on a comprehensive lunar noise temperature measurement campaign and associated theoretical treatment for a 34-m diameter Deep Space Network antenna observing an extended source such as the Moon. A set of measurements over a wide range of lunar phase angles was acquired at DSS-13, a 34-m diameter beam waveguide antenna (BWG) located at Goldstone, California at 2.3 GHz (S-band), 8.4 GHz (X-band) and 32 GHz (Ka-band). For validation purposes, independent predictions of noise temperature increase were derived using a physical optics characterization of the 34-m diameter antenna gain patterns and Apollo model-based brightness temperature maps of the Moon as input. The model-based predictions of noise temperature increase were compared with the measurements at all three frequencies. In addition, a methodology is presented that relates noise temperature increase due to the Moon to disk-centered or disk-averaged brightness temperature of the Moon at the microwave frequencies of interest. Comparisons were made between the measurements and models in the domain of lunar disk-centered and disk-averaged brightness temperatures. It is anticipated that the measurements and associated theoretical development will be useful in developing telecommunications strategies for future high-rate Ka-band communications where large diameter DSN antennas will be required. C1 [Morabito, David D.; Imbriale, William; Keihm, Stephen] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. RP Morabito, DD (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91125 USA. EM ddm@godzilla.jpl.nasa.gov NR 19 TC 9 Z9 12 U1 0 U2 2 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855 USA SN 0018-926X J9 IEEE T ANTENN PROPAG JI IEEE Trans. Antennas Propag. PD MAR PY 2008 VL 56 IS 3 BP 650 EP 660 DI 10.1109/TAP.2007.915471 PG 11 WC Engineering, Electrical & Electronic; Telecommunications SC Engineering; Telecommunications GA 274VB UT WOS:000254029300005 ER PT J AU Cheng, MK Nakashima, MA Moision, BE Harrikins, J AF Cheng, Michael K. Nakashima, Michael A. Moision, Bruce E. Harrikins, Jon TI Optimizations of a hardware decoder for deep-space optical communications SO IEEE TRANSACTIONS ON CIRCUITS AND SYSTEMS I-REGULAR PAPERS LA English DT Article DE cyclic redundancy check (CRC); field-programmable gate array (FPGA) implementation; optical communications; quadratic polynomial interleaver; turbo decoding ID PERMUTATION POLYNOMIALS; INTEGER RINGS; CODES; INTERLEAVERS AB The National Aeronautics and Space Administration has developed a capacity approaching modulation and coding scheme that comprises a serial concatenation of an inner accumulate pulse-position modulation (PPM) and an outer convolutional code [or serially concatenated PPM (SCPPM)] for deep-space optical communications. Decoding of this code uses the turbo principle. However, due to the nonbinary property of SCPPM, a straightforward application of classical turbo decoding is very inefficient. Here, we present various optimizations applicable in hardware implementation of the SCPPM decoder. More specifically, we feature a Super Gamma computation to efficiently handle parallel trellis edges, a pipeline-friendly "maxstar top-2" circuit that reduces the max-only approximation penalty, a low-latency cyclic redundancy check circuit for window-based decoders, and a high-speed algorithmic polynomial interleaver that leads to memory savings. Using the featured optimizations, we implement a 6.72 megabits-per-second (Mbps) SCPPM decoder on a single field-programmable gate array (FPGA). Compared to the current data rate of 256 kilobits per second from Mars, the SCPPM coded scheme represents a throughput increase of more than twenty-six fold. Extension to a 50-Mbps decoder on a board with multiple FPGAs follows naturally. We show through hardware simulations that the SCPPM coded system can operate within 1 dB of the Shannon capacity at nominal operating conditions. C1 [Cheng, Michael K.; Nakashima, Michael A.; Moision, Bruce E.; Harrikins, Jon] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Cheng, MK (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM mkcheng@jpl.nasa.gov NR 23 TC 11 Z9 12 U1 0 U2 2 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855 USA SN 1549-8328 J9 IEEE T CIRCUITS-I JI IEEE Trans. Circuits Syst. I-Regul. Pap. PD MAR PY 2008 VL 55 IS 2 BP 644 EP 658 DI 10.1109/TCSI.2007.913733 PG 15 WC Engineering, Electrical & Electronic SC Engineering GA 275KJ UT WOS:000254070000014 ER PT J AU Narasimham, B Shuler, RL Black, JD Bhuva, BL Schrimpf, RD Witulski, AF Holman, WT Massengill, LW AF Narasimham, Balaji Shuler, Robert L. Black, Jeffrey D. Bhuva, Bharat L. Schrimpf, Ronald D. Witulski, Arthur F. Holman, William Timothy Massengill, Lloyd W. TI Quantifying the reduction in collected charge and soft errors in the presence of guard rings SO IEEE TRANSACTIONS ON DEVICE AND MATERIALS RELIABILITY LA English DT Article DE collected charge; guard rings (GRs); pulse-width; radiation hardening by design (RHBD); single event (SE); SE transient (SET); soft error; soft-error rate (SER) ID MITIGATION AB Soft errors pose a major reliability threat to advanced electronic components and systems. Novel techniques are needed to mitigate the soft-error rate (SER) of integrated circuits (ICs), and in some cases, a combination of different mitigation techniques may be required for significant performance improvements. In this paper, an autonomous single-event-transient (SET) pulse-width characterization technique is used to quantify the effect of hardened-by-design structures, such as guard rings (GRs), in reducing the collected charge and SER of ICs. Experimental results obtained for a 0.35-mu m technology show a reduced SET pulse-width for devices with GRs; the corresponding reduction in SER was estimated to be greater than 55% for technologies ranging from 0.35 mu m to 70 nm. C1 [Narasimham, Balaji; Black, Jeffrey D.; Bhuva, Bharat L.; Schrimpf, Ronald D.; Witulski, Arthur F.; Holman, William Timothy; Massengill, Lloyd W.] Vanderbilt Univ, Nashville, TN 37235 USA. [Shuler, Robert L.] NASA, Lyndon B Johnson Space Ctr, Avion Syst Div, Houston, TX 77058 USA. RP Narasimham, B (reprint author), Vanderbilt Univ, 221 Kirkland Hall, Nashville, TN 37235 USA. EM balaji.narasimham@vanderbilt.edu RI Schrimpf, Ronald/L-5549-2013 OI Schrimpf, Ronald/0000-0001-7419-2701 NR 11 TC 7 Z9 8 U1 0 U2 1 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 1530-4388 EI 1558-2574 J9 IEEE T DEVICE MAT RE JI IEEE Trans. Device Mater. Reliab. PD MAR PY 2008 VL 8 IS 1 BP 203 EP 209 DI 10.1109/TDMR.2007.912778 PG 7 WC Engineering, Electrical & Electronic; Physics, Applied SC Engineering; Physics GA 275KF UT WOS:000254069600022 ER PT J AU Kerr, YH Le Vine, DM AF Kerr, Yann H. Le Vine, David M. TI Foreword to the special issue on the Soil Moisture and Ocean Salinity (SMOS) mission SO IEEE TRANSACTIONS ON GEOSCIENCE AND REMOTE SENSING LA English DT Editorial Material ID APERTURE MICROWAVE RADIOMETER; RETRIEVAL; SPACE; ESTAR C1 [Kerr, Yann H.] CESBIO, F-31401 Toulouse, France. [Le Vine, David M.] NASA, Goddard Space Flight Ctr, Instrumentat Sci Branch, Greenbelt, MD 20771 USA. RP Kerr, YH (reprint author), CESBIO, F-31401 Toulouse, France. NR 19 TC 8 Z9 9 U1 0 U2 4 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855 USA SN 0196-2892 J9 IEEE T GEOSCI REMOTE JI IEEE Trans. Geosci. Remote Sensing PD MAR PY 2008 VL 46 IS 3 BP 583 EP 585 DI 10.1109/TGRS.2008.917807 PG 3 WC Geochemistry & Geophysics; Engineering, Electrical & Electronic; Remote Sensing; Imaging Science & Photographic Technology SC Geochemistry & Geophysics; Engineering; Remote Sensing; Imaging Science & Photographic Technology GA 270QB UT WOS:000253734200001 ER PT J AU Panciera, R Walker, JP Kalma, JD Kim, EJ Hacker, JM Merlin, O Berger, M Skou, N AF Panciera, Rocco Walker, Jeffrey P. Kalma, Jetse D. Kim, Edward J. Hacker, Joerg M. Merlin, Olivier Berger, Michael Skou, Niels TI The NAFE'05/CoSMOS data set: Toward SMOS soil moisture retrieval, downscaling, and assimilation SO IEEE TRANSACTIONS ON GEOSCIENCE AND REMOTE SENSING LA English DT Article DE microwave radiometry; National Airborne Field Experiment (NAFE); passive microwave; soil moisture; Soil Moisture and Ocean Salinity (SMOS) ID MODEL; BAND AB The National Airborne Field Experiment 2005 (NAFE'05) and the Campaign for validating the Operation of Soil Moisture and Ocean Salinity (COSMOS) were undertaken in November 2005 in the Goulburn River catchment, which is located in southeastern Australia. The objective of the joint campaign was to provide simulated Soil Moisture and Ocean Salinity (SMOS) observations using airborne L-band radiometers supported by soil moisture and other relevant ground data for the following: 1) the development of SMOS soil moisture retrieval algorithms; 2) developing approaches for downscaling the low-resolution data from SMOS; and 3) testing its assimilation into land surface models for root zone soil moisture retrieval. This paper describes the NAFE'05 and COSMOS airborne data sets together with the ground data collected in support of both aircraft campaigns. The airborne L-band acquisitions included 40 km x 40 km coverage flights at 500-m and 1-km resolution for the simulation of a SMOS pixel, multiresolution flights with ground resolution ranging from 1 km to 62.5 m, multiangle observations, and specific flights that targeted the vegetation dew and sun glint effect on L-band soil moisture retrieval. The L-band data were accompanied by airborne thermal infrared and optical measurements. The ground data consisted of continuous soil moisture profile measurements at 18 monitoring sites throughout the 40 km x 40 km study area and extensive spatial near-surface soil moisture measurements concurrent with airborne monitoring. Additionally, data were collected on rock coverage and temperature, surface roughness, skin and soil temperatures, dew amount, and vegetation water content and biomass. These data are available at www.nafe.unimelb. edu.au. C1 [Panciera, Rocco; Walker, Jeffrey P.; Merlin, Olivier] Univ Melbourne, Dept Civil & Environm Engn, Melbourne, Vic 3010, Australia. [Kalma, Jetse D.] Univ Newcastle, Sch Engn, Callaghan, NSW 2308, Australia. [Kim, Edward J.] NASA, Hydrospher & Biospher Sci Lab, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Hacker, Joerg M.] Airborne Res Australia, Salisbury, SA 5106, Australia. [Berger, Michael] European Space Agcy, Earth Observat Ctr, ESRIN, Sci Strategy Coordinat & Planning Off EOP SA, I-00044 Frascati, Italy. [Skou, Niels] Tech Univ Denmark, DK-2800 Lyngby, Denmark. [Skou, Niels] Danish Natl Space Ctr, DK-2100 Copenhagen, Denmark. [Hacker, Joerg M.] Flinders Univ S Australia, Adelaide, SA 5001, Australia. RP Panciera, R (reprint author), Univ Melbourne, Dept Civil & Environm Engn, Melbourne, Vic 3010, Australia. EM rocco@civenv.unimelb.edu.au RI Walker, Jeffrey/D-2624-2009 NR 18 TC 64 Z9 66 U1 0 U2 11 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 0196-2892 EI 1558-0644 J9 IEEE T GEOSCI REMOTE JI IEEE Trans. Geosci. Remote Sensing PD MAR PY 2008 VL 46 IS 3 BP 736 EP 745 DI 10.1109/TGRS.2007.915403 PG 10 WC Geochemistry & Geophysics; Engineering, Electrical & Electronic; Remote Sensing; Imaging Science & Photographic Technology SC Geochemistry & Geophysics; Engineering; Remote Sensing; Imaging Science & Photographic Technology GA 270QB UT WOS:000253734200015 ER PT J AU Marquette, ML Byerly, D Sognier, M AF Marquette, Michele L. Byerly, Diane Sognier, Marguerite TI The effects of three-dimensional cell culture on single myoblasts SO IN VITRO CELLULAR & DEVELOPMENTAL BIOLOGY-ANIMAL LA English DT Article DE myoblast; 3D; three dimensional; skeletal muscle; F-actin; podia ID PROSTATE-CANCER CELLS; ELECTRON-MICROSCOPY; DEPENDENT CONTROL; GENE-EXPRESSION; LATRUNCULIN-A; APOPTOSIS; GROWTH; DIFFERENTIATION; FIBROBLASTS; ADHESION AB Identification of cellular and morphological changes in myoblasts during three-dimensional (3D) culture may provide novel insight into skeletal muscle morphogenesis. One particular morphological change that occurs during the transition from monolayer culture to the 3D environment is the appearance of cytoplasmic projections (podia). The purpose of these studies was to determine if: (1) 3D culture increased podia formation in single cells, and (2) podia were F-actin dependent. C2C12 cells were grown in 3D conditions using a rotary cell culture system (RCCS) for 3, 6, and 9 h, fixed, and stained. Analysis of confocal images revealed that podia were significantly more numerous on RCCS cultured cells than those on suspension controls. Further, the podia of RCCS cultured cells decreased in number and increased in length during the time intervals examined. RCCS cultured cells showed no significant changes in viability, Annexin V staining, and activated Caspase 3 expression over time. In contrast, significant decreases in viability of suspension controls occurred. The application of 2 mu M Latrunculin A (Lat A), an actin depolymerizing agent, significantly reduced the number of cells with podia. The number of cells with podia recovered with Lat A removal. Changes in viability and apoptosis markers were not significant during Lat A application or washout experiments. These observations reveal that: (1) culture conditions in the RCCS increase the quantity of podia formation; (2) these podia increase in length with time; and (3) F-actin plays a role in podia formation. C1 [Marquette, Michele L.; Byerly, Diane] NASA, Lyndon B Johnson Space Ctr, ORAU, Houston, TX 77058 USA. [Sognier, Marguerite] USRA, Houston, TX 77058 USA. RP Marquette, ML (reprint author), NASA, Lyndon B Johnson Space Ctr, ORAU, 2101 NASA Rd 1, Houston, TX 77058 USA. EM michele.marquette-1@nasa.gov NR 38 TC 3 Z9 3 U1 0 U2 1 PU SPRINGER PI NEW YORK PA 233 SPRING STREET, NEW YORK, NY 10013 USA SN 1071-2690 J9 IN VITRO CELL DEV-AN JI In Vitro Cell. Dev. Biol.-Anim. PD MAR-APR PY 2008 VL 44 IS 3-4 BP 105 EP 114 DI 10.1007/s11626-007-9078-5 PG 10 WC Cell Biology; Developmental Biology SC Cell Biology; Developmental Biology GA 283GE UT WOS:000254623900009 PM 18246406 ER PT J AU Jordan, JA Verhoff, AM Fischer, DG AF Jordan, J. A. Verhoff, A. M. Fischer, D. G. TI Assessing the in vitro respiratory toxicity of fine particles of Al2O3 and SiO2: A precursor study for lunar dust toxicity SO IN VITRO CELLULAR & DEVELOPMENTAL BIOLOGY-ANIMAL LA English DT Meeting Abstract C1 NASA, Glenn Res Ctr, Biosci & Technol Branch, Cleveland, OH 44135 USA. Clayton State Univ, Dept Nat Sci, Morrow, GA 30260 USA. EM dgfisher@nasa.gov NR 0 TC 0 Z9 0 U1 0 U2 3 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 1071-2690 J9 IN VITRO CELL DEV-AN JI In Vitro Cell. Dev. Biol.-Anim. PD SPR PY 2008 VL 44 SU S BP S48 EP S48 PG 1 WC Cell Biology; Developmental Biology SC Cell Biology; Developmental Biology GA 338XL UT WOS:000258542600123 ER PT J AU O'Sullivan, C Cahill, G Murphy, JA Gear, WK Harris, J Ade, PAR Church, SE Thompson, KL Pryke, C Bock, J Bowden, M Brown, ML Carlstrom, JE Castro, PG Culverhouse, T Friedman, RB Ganga, KM Haynes, V Hinderks, JR Kovak, J Lange, AE Leitch, EM Mallie, OE Melhuish, SJ Orlando, A Piccirillo, L Pisano, G Rajguru, N Rusholme, BA Schwarz, R Taylor, AN Wu, EYS Zemcov, M AF O'Sullivan, C. Cahill, G. Murphy, J. A. Gear, W. K. Harris, J. Ade, P. A. R. Church, S. E. Thompson, K. L. Pryke, C. Bock, J. Bowden, M. Brown, M. L. Carlstrom, J. E. Castro, P. G. Culverhouse, T. Friedman, R. B. Ganga, K. M. Haynes, V. Hinderks, J. R. Kovak, J. Lange, A. E. Leitch, E. M. Mallie, O. E. Melhuish, S. J. Orlando, A. Piccirillo, L. Pisano, G. Rajguru, N. Rusholme, B. A. Schwarz, R. Taylor, A. N. Wu, E. Y. S. Zemcov, M. TI The quasi-optical design of the QUaD telescope SO INFRARED PHYSICS & TECHNOLOGY LA English DT Article DE quasioptics; gaussian beam modes; optical design; feedhorn design; cosmic microwave background ID CMB POLARIZATION EXPERIMENT; CORRUGATED HORNS; MILLIMETER-WAVE; DASI AB We describe the optical design and performance of 'QUEST and DASI' or 'QUaD', a ground-based high-resolution experiment designed to measure the polarisation properties of the cosmic microwave background radiation. QUaD uses bolometric detectors at 100 and 150 GHz on a 2.6 m Cassegrain telescope. The QUaD optics are designed to minimise systematic effects as well as to maximise sensitivity, and we report here on the comprehensive quasi-optical analysis used to achieve this design. We also present initial optical performance measurements achieved in operation, and discuss changes made to the optics to overcome some errors in the mechanical construction of the primary mirror. The QUaD experiment is now fully operational and taking world-leading data at the South Pole. (C) 2007 Elsevier B.V. All rights reserved. C1 [O'Sullivan, C.; Cahill, G.; Murphy, J. A.] Natl Univ Ireland Maynooth, Dept Expt Phys, Kildare, Ireland. [Gear, W. K.; Harris, J.; Ade, P. A. R.; Bowden, M.; Haynes, V.; Mallie, O. E.; Melhuish, S. J.; Orlando, A.; Piccirillo, L.; Pisano, G.; Rajguru, N.; Zemcov, M.] Cardiff Univ, Sch Phys & Astron, Cardiff CF24 3AA, S Glam, Wales. [Church, S. E.; Thompson, K. L.; Bowden, M.; Hinderks, J. R.; Rusholme, B. A.; Wu, E. Y. S.] Stanford Univ, Dept Phys, Stanford, CA 94305 USA. [Church, S. E.; Thompson, K. L.; Bowden, M.; Hinderks, J. R.; Rusholme, B. A.; Wu, E. Y. S.] Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, Stanford, CA 94305 USA. [Pryke, C.; Carlstrom, J. E.; Culverhouse, T.; Friedman, R. B.; Schwarz, R.] Univ Chicago, Kavli Inst Cosmol Phys, Dept Astron & Astrophys, Enrico Fermi Inst, Chicago, IL 60637 USA. [Bock, J.; Leitch, E. M.; Zemcov, M.] Jet Prop Lab, Pasadena, CA 91109 USA. [Bock, J.; Kovak, J.; Lange, A. E.; Leitch, E. M.; Zemcov, M.] CALTECH, Pasadena, CA 91125 USA. [Brown, M. L.; Castro, P. G.] Univ Edinburgh, Royal Observ, Inst Astron, Edinburgh EH9 3HJ, Midlothian, Scotland. [Ganga, K. M.] CNRS, Lab APC, F-75205 Paris 13, France. RP O'Sullivan, C (reprint author), Natl Univ Ireland Maynooth, Dept Expt Phys, Kildare, Ireland. EM creidhe.osullivan@nuim.ie RI Melhuish, Simon/B-1299-2016; OI Melhuish, Simon/0000-0001-8725-4991; Orlando, Angiola/0000-0001-8004-5054 NR 21 TC 12 Z9 12 U1 0 U2 1 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 1350-4495 J9 INFRARED PHYS TECHN JI Infrared Phys. Technol. PD MAR PY 2008 VL 51 IS 4 BP 277 EP 286 DI 10.1016/j.infrared.2007.10.001 PG 10 WC Instruments & Instrumentation; Optics; Physics, Applied SC Instruments & Instrumentation; Optics; Physics GA 288KA UT WOS:000254984100001 ER PT J AU Biswas, R Oliker, L AF Biswas, Rupak Oliker, Leonid TI Special issue on performance characterization of the world's most powerful supercomputers - Part 1 - Preface SO INTERNATIONAL JOURNAL OF HIGH PERFORMANCE COMPUTING APPLICATIONS LA English DT Editorial Material C1 [Biswas, Rupak] NASA, Ames Res Ctr, NAS Div, Moffett Field, CA 94035 USA. [Oliker, Leonid] Lawrence Berkeley Natl Lab, NERSC, CRD, Berkeley, CA 94720 USA. RP Biswas, R (reprint author), NASA, Ames Res Ctr, NAS Div, Moffett Field, CA 94035 USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU SAGE PUBLICATIONS LTD PI LONDON PA 1 OLIVERS YARD, 55 CITY ROAD, LONDON EC1Y 1SP, ENGLAND SN 1094-3420 J9 INT J HIGH PERFORM C JI Int. J. High Perform. Comput. Appl. PD SPR PY 2008 VL 22 IS 1 BP 3 EP 4 DI 10.1177/10943420070085013 PG 2 WC Computer Science, Hardware & Architecture; Computer Science, Interdisciplinary Applications; Computer Science, Theory & Methods SC Computer Science GA 270LZ UT WOS:000253723600001 ER PT J AU Hood, R Biswas, R Chang, J Djornehri, MJ Jin, H AF Hood, Robert Biswas, Rupak Chang, Johnny Djornehri, M. Jahed Jin, Haoqiang TI Benchmarking the Columbia supercluster SO INTERNATIONAL JOURNAL OF HIGH PERFORMANCE COMPUTING APPLICATIONS LA English DT Article DE SGI altix; HPC challenge benchmarks; NAS parallel benchmarks; computational fluid dynamics AB Columbia, NASA's 10,240-processor supercluster, has been ranked as one of the fastest computers in the world since November 2004. In this paper we examine the performance characteristics of its production subclusters, which are typically configurations ranging in size from 512 to 2048 processors. We evaluate floating-point performance, memory bandwidth, and message passing communication speeds using a subset of the HPC Challenge benchmarks, the NAS Parallel Benchmarks, and a computational fluid dynamics application. Our experimental results quantify the performance improvement resulting from changes in interconnect bandwidth, processor speed, and cache size across the different types of SGI Altix 3700s that constitute Columbia. We also report on our experiments that investigate the performance impact of processors sharing a path to memory. Finally, our tests of the different interconnect fabrics available indicate substantial promise for scaling applications to run on configurations of more than 512 CPUs. C1 [Hood, Robert; Biswas, Rupak; Chang, Johnny; Djornehri, M. Jahed; Jin, Haoqiang] NASA, Ames Res Ctr, NASA Adv Supercomp NAS Div, Moffett Field, CA 94035 USA. RP Hood, R (reprint author), NASA, Ames Res Ctr, NASA Adv Supercomp NAS Div, Moffett Field, CA 94035 USA. EM RHOOD@MAIL.ARC.NASA.GOV NR 15 TC 0 Z9 0 U1 0 U2 0 PU SAGE PUBLICATIONS LTD PI LONDON PA 1 OLIVERS YARD, 55 CITY ROAD, LONDON EC1Y 1SP, ENGLAND SN 1094-3420 J9 INT J HIGH PERFORM C JI Int. J. High Perform. Comput. Appl. PD SPR PY 2008 VL 22 IS 1 BP 97 EP 112 DI 10.1177/1094342006085021 PG 16 WC Computer Science, Hardware & Architecture; Computer Science, Interdisciplinary Applications; Computer Science, Theory & Methods SC Computer Science GA 270LZ UT WOS:000253723600007 ER PT J AU Nakano, A Kalia, RK Nomura, KI Sharma, A Vashishta, P Shimojo, F Van Duin, ACT Goddard, WA Biswas, R Srivastava, D Yang, LH AF Nakano, Aiichiro Kalia, Rajiv K. Nomura, Ken-Ichi Sharma, Ashish Vashishta, Priya Shimojo, Fuyuki Van Duin, Adri C. T. Goddard, William A., III Biswas, Rupak Srivastava, Deepak Yang, Lin H. TI De novo ultrascale atomistic simulations on high-end parallel supercomputers SO INTERNATIONAL JOURNAL OF HIGH PERFORMANCE COMPUTING APPLICATIONS LA English DT Article DE hierarchical simulation; molecular dynamics; reactive force field; quantum mechanics; density functional theory; parallel computing; grid computing ID MOLECULAR-DYNAMICS SIMULATIONS; DENSITY-FUNCTIONAL THEORY; ELECTRONIC-STRUCTURE METHODS; COMPUTATIONAL CHEMISTRY; SPACE; COMPUTERS; ALGORITHM; IMPLEMENTATION; OXIDATION; CERAMICS AB We present a de novo, hierarchical simulation framework for first-principles based predictive simulations of materials and their validation on high-end parallel supercomputers and geographically distributed clusters. In this framework, high-end chemically reactive and non-reactive molecular dynamics (MID) simulations explore a wide solution space to discover microscopic mechanisms that govern macroscopic material properties, into which highly accurate quantum mechanical (QM) simulations are embedded to validate the discovered mechanisms and quantify the uncertainty of the solution. The framework includes an embedded divide-and conquer (EDC) algorithmic framework for the design of linear-scaling simulation algorithms with minimal bandwidth complexity and tight error control. The EDC framework also enables adaptive hierarchical simulation with automated model transitioning assisted by graph-based event tracking. A tunable hierarchical cellular decomposition parallelization framework then maps the O(N) EDC algorithms onto petaflops computers, while achieving performance tunability through a hierarchy of parameterized cell data/ computation structures, as well as its implementation using hybrid grid remote procedure call + message passing + threads programming. High-end computing platforms such as IBM BlueGene/L, SGI Altix 3000 and the NSF TeraGrid provide an excellent test grounds for the framework. On these platforms, we have achieved unprecedented scales of quantum-mechanically accurate and well validated, chemically reactive atomistic simulations-1.06 billion-atom fast reactive force-field MID and 11.8 million-atom (1.04 trillion grid points) quantum-mechanical MID in the framework of the EDC density functional theory on adaptive multigrids-in addition to 134 billion-atom non-reactive space-time multiresolution MD, with the parallel efficiency as high as 0.998 on 65,536 dual-processor BlueGene/L nodes. We have also achieved an automated execution of hierarchical QM/MD simulation on a grid consisting of 6 supercomputer centers in the US and Japan (in total of 150,000 processor hours), in which the number of processors change dynamically on demand and resources are allocated and migrated dynamically in response to faults. Furthermore, performance portability has been demonstrated on a wide range of platforms such as BlueGene/L, Altix 3000, and AMD Opteron-based Linux clusters. C1 [Nakano, Aiichiro; Kalia, Rajiv K.; Nomura, Ken-Ichi; Sharma, Ashish; Vashishta, Priya; Shimojo, Fuyuki] Univ So Calif, Collaborat Adv Comp & Simulat, Los Angeles, CA 90089 USA. [Sharma, Ashish] Ohio State Univ, Dept Biomed Informat, Columbus, OH 43210 USA. [Van Duin, Adri C. T.] Kumamoto Univ, Fac Gen Educ, Dept Phys, Kumamoto 8608555, Japan. [Van Duin, Adri C. T.; Goddard, William A., III] CALTECH, Mat & Proc Simulat Ctr, Pasadena, CA 91125 USA. [Biswas, Rupak; Srivastava, Deepak] NASA, Ames Res Ctr, NASA Adv Supercomp NAS Div, Moffett Field, CA 94035 USA. [Yang, Lin H.] Lawrence Livermore Natl Lab, Phys H Div, Livermore, CA 94551 USA. RP Nakano, A (reprint author), Univ So Calif, Collaborat Adv Comp & Simulat, Los Angeles, CA 90089 USA. EM ANAKANO@USC.EDU NR 58 TC 30 Z9 30 U1 2 U2 13 PU SAGE PUBLICATIONS LTD PI LONDON PA 1 OLIVERS YARD, 55 CITY ROAD, LONDON EC1Y 1SP, ENGLAND SN 1094-3420 EI 1741-2846 J9 INT J HIGH PERFORM C JI Int. J. High Perform. Comput. Appl. PD SPR PY 2008 VL 22 IS 1 BP 113 EP 128 DI 10.1177/1094342007085015 PG 16 WC Computer Science, Hardware & Architecture; Computer Science, Interdisciplinary Applications; Computer Science, Theory & Methods SC Computer Science GA 270LZ UT WOS:000253723600008 ER PT J AU Hull, DH Harries, KA AF Hull, Daniel H. Harries, Kent A. TI On the applicability of fixed point theory to the behavior of coupled core walls SO INTERNATIONAL JOURNAL OF STRUCTURAL STABILITY AND DYNAMICS LA English DT Article DE coupled walls; dynamic behavior; fixed point theory; structural optimization ID DESIGN AB The performance-based design of coupled core wall systems offers a number of advantages over conventional strength-based methods in terms of constructability and structural performance. Under large seismic loads, the expected degradation of the coupling beams in coupled wall structures results in an evolution of the lateral force resisting system from a coupled wall system to a system of linked cantilever wall piers. The present study focuses on the performance of the eventually obtained linked wall pier systems and defines their performance in a novel way: as the minimization of transmissibility of horizontal ground motion. In this paper, fixed point theory (FPT) is used to establish initial design values for the coupling beams required to optimize the dynamic response of the linked wall pier system. An initial parametric study of the application of FPT to optimizing the behavior of linked wall piers is presented. The resulting optimized wall systems are compared with practically obtainable, rigid and uncoupled systems subject to a linear time history analysis to assess the extent and practicality of optimization obtained. C1 [Hull, Daniel H.] NASA, Kennedy Space Ctr, FL 32899 USA. [Harries, Kent A.] Univ Pittsburgh, Dept Civil & Environm Engn, Pittsburgh, PA 15261 USA. RP Hull, DH (reprint author), NASA, Kennedy Space Ctr, FL 32899 USA. EM kharries@pitt.edu OI Harries, Kent/0000-0002-8421-2523 NR 17 TC 4 Z9 4 U1 0 U2 2 PU WORLD SCIENTIFIC PUBL CO PTE LTD PI SINGAPORE PA 5 TOH TUCK LINK, SINGAPORE 596224, SINGAPORE SN 0219-4554 J9 INT J STRUCT STAB DY JI Int. J. Struct. Stab. Dyn. PD MAR PY 2008 VL 8 IS 1 BP 161 EP 186 DI 10.1142/S0219455408002594 PG 26 WC Engineering, Civil; Engineering, Mechanical; Mechanics SC Engineering; Mechanics GA 278NF UT WOS:000254292900009 ER PT J AU McKay, TL Gedeon, DJ Vickerman, MB Hylton, AG Ribita, D Olar, HH Kaiser, PK Parsons-Wingerter, P AF McKay, Terri L. Gedeon, Dan J. Vickerman, Mary B. Hylton, Alan G. Ribita, Daniela Olar, Harry H. Kaiser, Peter K. Parsons-Wingerter, Patricia TI Selective inhibition of angiogenesis in small blood vessels and decrease in vessel diameter throughout the vascular tree by triamcinolone acetonide SO INVESTIGATIVE OPHTHALMOLOGY & VISUAL SCIENCE LA English DT Article ID ENDOTHELIAL GROWTH-FACTOR; INTRAVITREAL TRIAMCINOLONE; MORPHOMETRY; EXPRESSION; VEGF AB PURPOSE. To quantify the effects of the steroid triamcinolone acetonide (TA) on branching morphology within the angiogenic microvascular tree of the chorioallantoic membrane (CAM) of quail embryos. METHODS. Increasing concentrations of TA (0-16 ng/mL) were applied topically on embryonic day (E) 7 to the chorioallantoic membrane (CAM) of quail embryos cultured in petri dishes and incubated for an additional 24 or 48 hours until fixation. Binary (black/white) microscopic images of arterial end points were quantified by generational analysis of vessel branching (VESGEN) software to obtain major vascular parameters that include vessel diameter (D-v), fractal dimension (D-f), tortuosity (T-v), and densities of vessel area, length, number, and branch point (A(v), L-v, N-v, and Br-v). For assessment of specific changes in vascular morphology induced by TA, the VESGEN software automatically segmented the vascular tree into branching generations (G(1)... G(10)) according to changes in vessel diameter and branching. RESULTS. Vessel density decreased significantly up to 34% as the function of increasing concentration of TA according to A(v), L-v, Br-v, N-v, and D-f. TA selectively inhibited the growth of new, small vessels because L v decreased from 13.14 +/- 0.61 cm/cm(2) for controls to 8.012 +/- 0.82 cm/cm(2) at 16 ng TA/mL in smaller branching generations (G(7)-G(10)) and for N v from 473.83 +/- 29.85 cm(-2) to 302.32 +/- 33.09 cm(-2). In contrast, vessel diameter (D v) decreased throughout the vascular tree (G(1)-G(10)). CONCLUSIONS. By VESGEN analysis, TA selectively inhibited the angiogenesis of smaller blood vessels, but decreased the vessel diameter of all vessels within the vascular tree. C1 [McKay, Terri L.; Gedeon, Dan J.; Vickerman, Mary B.; Hylton, Alan G.; Ribita, Daniela; Olar, Harry H.; Parsons-Wingerter, Patricia] NASA, Glenn Res Ctr, Res Technol & Directorate, Cleveland, OH 44135 USA. [McKay, Terri L.; Gedeon, Dan J.; Vickerman, Mary B.; Hylton, Alan G.; Ribita, Daniela; Olar, Harry H.; Parsons-Wingerter, Patricia] NASA, Glenn Res Ctr, Natl Ctr Space Explorat Res, Cleveland, OH 44135 USA. [Kaiser, Peter K.] Cole Eye Inst, Cleveland Clin Fdn, Cleveland, OH 44195 USA. RP Parsons-Wingerter, P (reprint author), NASA, Glenn Res Ctr, Res Technol & Directorate, MS 110-3, Cleveland, OH 44135 USA. EM patricia.parsons@grc.nasa.gov FU NEI NIH HHS [R01EY17529, R01EY17528] NR 26 TC 19 Z9 20 U1 0 U2 0 PU ASSOC RESEARCH VISION OPHTHALMOLOGY INC PI ROCKVILLE PA 12300 TWINBROOK PARKWAY, ROCKVILLE, MD 20852-1606 USA SN 0146-0404 J9 INVEST OPHTH VIS SCI JI Invest. Ophthalmol. Vis. Sci. PD MAR PY 2008 VL 49 IS 3 BP 1184 EP 1190 DI 10.1167/iovs.07-1329 PG 7 WC Ophthalmology SC Ophthalmology GA 271TZ UT WOS:000253812900050 PM 18326748 ER PT J AU Di, KC Xu, FL Wang, J Agarwal, S Brodyagina, E Li, RX Matthies, L AF Di, Kaichang Xu, Fengliang Wang, Jue Agarwal, Sanchit Brodyagina, Evgenia Li, Rongxing Matthies, Larry TI Photogrammetric processing of rover imagery of the 2003 Mars Exploration Rover mission SO ISPRS JOURNAL OF PHOTOGRAMMETRY AND REMOTE SENSING LA English DT Article DE Mars rover; topographic mapping; rover localization; incremental bundle adjustment; tie point selection ID LANDING-SITE; LOCALIZATION; CAMERAS; SYSTEM AB In the 2003 Mars Exploration Rover (MER) mission, the twin rovers, Spirit and Opportunity, carry identical Athena instrument payloads and engineering cameras for exploration of the Gusev Crater and Meridiani Planum landing sites. This paper presents the photogrammetric processing techniques for high accuracy topographic mapping and rover localization at the two landing sites. Detailed discussions about camera models, reference frames, interest point matching, automatic tie point selection, image network construction, incremental bundle adjustment, and topographic product generation are given. The developed rover localization method demonstrated the capability of correcting position errors caused by wheel slippages, azimuthal angle drift and other navigation errors. A comparison was also made between the bundle-adjusted rover traverse and the rover track imaged from the orbit. Mapping products including digital terrain models, orthophotos, and rover traverse maps have been generated for over two years of operations, and disseminated to scientists and engineers of the mission through a web-based GIS. The maps and localization information have been extensively used to support tactical operations and strategic planning of the mission. (C) 2007 International Society for Photogrammetry and Remote Sensing, Inc. (ISPRS). Published by Elsevier B.V. All rights reserved. C1 [Di, Kaichang; Xu, Fengliang; Wang, Jue; Agarwal, Sanchit; Brodyagina, Evgenia; Li, Rongxing] Ohio State Univ, Dept Civil & Environm Engn & Geodet Sci, Mapping & GIS Lab, Columbus, OH 43210 USA. [Matthies, Larry] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Li, RX (reprint author), Ohio State Univ, Dept Civil & Environm Engn & Geodet Sci, Mapping & GIS Lab, 470 Hitchcock Hall,2070 Neil Ave, Columbus, OH 43210 USA. EM li.282@osu.edu RI Wang, Jue/C-9215-2009; OI Wang, Jue/0000-0002-9901-9996; di, kai chang/0000-0001-6581-6615 NR 47 TC 16 Z9 26 U1 1 U2 13 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0924-2716 EI 1872-8235 J9 ISPRS J PHOTOGRAMM JI ISPRS-J. Photogramm. Remote Sens. PD MAR PY 2008 VL 63 IS 2 BP 181 EP 201 DI 10.1016/j.isprsjprs.2007.07.007 PG 21 WC Geography, Physical; Geosciences, Multidisciplinary; Remote Sensing; Imaging Science & Photographic Technology SC Physical Geography; Geology; Remote Sensing; Imaging Science & Photographic Technology GA 283TY UT WOS:000254660600003 ER PT J AU Consiglio, MC Carreno, V Williams, DM Munoz, C AF Consiglio, Maria C. Carreno, Victor Williams, Daniel M. Munoz, Cesar TI Conflict prevention and separation assurance in Small Aircraft Transportation Systems SO JOURNAL OF AIRCRAFT LA English DT Article; Proceedings Paper CT AIAA 5th Aviation, Technology, Integration, and Operations Conference (ATIO) CY SEP 26-28, 2005 CL Arlington, VA SP AIAA AB A multilayer approach to the prevention of conflicts due to the loss of aircraft-to-aircraft separation that relies on procedures and onboard automation was implemented as part of the Small Aircraft Transportation Systems Higher-Volume-Operations concept. The multilayer system gives pilots support and guidance during the execution of normal operations and advance warning for procedure deviations or off-nominal operations. This paper describes the major concept elements of this multilayer approach to separation assurance and conflict prevention and provides the rationale for its design. All the algorithms and functionality described in this paper were implemented in an aircraft simulation in the Air Traffic Operations Laboratory at NASA Langley Research Center and on the NASA Cirrus SR22 research aircraft. C1 [Consiglio, Maria C.] NASA, Langley Res Ctr, Crew Syst Branch, Hampton, VA 23681 USA. [Carreno, Victor] NASA, Langley Res Ctr, Safety Crit Avionics Syst Branch, Hampton, VA 23681 USA. [Williams, Daniel M.] NASA, Langley Res Ctr, Aviat Operat & Evaluat Branch, Hampton, VA 23681 USA. [Munoz, Cesar] Natl Inst Aerosp, Format Methods Team, Hampton, VA 23666 USA. RP Consiglio, MC (reprint author), NASA, Langley Res Ctr, Crew Syst Branch, 24 W Taylor St,Mail Stop 152, Hampton, VA 23681 USA. NR 17 TC 8 Z9 8 U1 0 U2 1 PU AMER INST AERONAUT ASTRONAUT PI RESTON PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA SN 0021-8669 J9 J AIRCRAFT JI J. Aircr. PD MAR-APR PY 2008 VL 45 IS 2 BP 353 EP 358 DI 10.2514/1.20586 PG 6 WC Engineering, Aerospace SC Engineering GA 285FB UT WOS:000254761600001 ER PT J AU Consiglio, MC Williams, DM Murdoch, JL Adams, CA AF Consiglio, Maria C. Williams, Daniel M. Murdoch, Jennifer L. Adams, Catherine A. TI Concept validation experiment for small aircraft transportation system higher-volume operations SO JOURNAL OF AIRCRAFT LA English DT Article; Proceedings Paper CT AIAA 5th Aviation, Technology, Integration, and Operations Conference (ATIO) CY SEP 26-28, 2005 CL Arlington, VA SP AIAA AB A human-in-the-loop simulation experiment was conducted at the NASA Langley Research Center's Air Traffic Operations Laboratory in an effort to comprehensively validate tools and procedures intended to enable the small aircraft transportation system higher-volume-operations concept of operations. These procedures were developed with the goal of increasing the rate of operations at nontowered, nonradar airports in near all-weather conditions. A key element of the new design is the establishment of a volume of airspace around designated airports at which pilots accept responsibility for self-separation. Flights operating at these airports are given approach-sequencing information computed by a ground-based automated system. The validation experiment was conducted to determine if a pilot could safety and proficiently fly an airplane while performing the newly developed procedures. Comparative measures of flight path error, perceived workload, and situation awareness were obtained for two types of simulated scenarios. Baseline scenarios were representative of today's system using procedure separation, in which air traffic control grants one approach or departure clearance at a time. Test scenarios represented the newly developed approach and departure procedures. Results from the experiment indicate that low-time pilots were able to fly the test procedures in a simulation environment and maintain self-separation as safely and proficiently as flying today's procedures. C1 [Consiglio, Maria C.; Adams, Catherine A.] NASA, Langley Res Ctr, Crew Syst Branch, Hampton, VA 23681 USA. [Williams, Daniel M.; Murdoch, Jennifer L.] NASA, Langley Res Ctr, Aviat Operat & Evaluat Branch, Hampton, VA 23681 USA. RP Consiglio, MC (reprint author), NASA, Langley Res Ctr, Crew Syst Branch, 24 W Taylor St,Mail Stop 152, Hampton, VA 23681 USA. NR 15 TC 2 Z9 2 U1 0 U2 2 PU AMER INST AERONAUT ASTRONAUT PI RESTON PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA SN 0021-8669 J9 J AIRCRAFT JI J. Aircr. PD MAR-APR PY 2008 VL 45 IS 2 BP 359 EP 365 DI 10.2514/1.20588 PG 7 WC Engineering, Aerospace SC Engineering GA 285FB UT WOS:000254761600002 ER PT J AU Davila, CG Camanho, PP Turon, A AF Davila, Carlos G. Camanho, Pedro P. Turon, Albert TI Effective simulation of delamination in aeronautical structures using shells and cohesive elements SO JOURNAL OF AIRCRAFT LA English DT Article ID ENERGY-RELEASE RATE; PLATE ELEMENTS; ZONE MODEL; FRACTURE; COMPUTATION; COMPOSITES; TOUGHNESS; STRESSES; GROWTH; CRACK AB A cohesive element for shell analysis is presented. The element can be used to simulate the initiation and growth of delaminations between stacked noncoincident layers of shell elements. The procedure to construct the element accounts for the thickness offset by applying the kinematic relations of shell deformation to transform the stiffness and internal force of a zero-thickness cohesive element such that interfacial continuity between the layers is enforced. The procedure is demonstrated by simulating the response and failure of the mixed-mode bending test and a skin-stiffener debond specimen. In addition, it is shown that stacks of shell elements can be used to create effective models to predict the in-plane and delamination failure modes of thick components. The results indicate that simple shell models can retain many of the necessary predictive attributes of much more complex three-dimensional models while providing the computational efficiency that is necessary for design. C1 [Davila, Carlos G.] NASA, Langley Res Ctr, Durabil Damage Tolerance & Reliabil Branch, Hampton, VA 23602 USA. [Camanho, Pedro P.] Univ Porto, Fac Engn, Dept Engn Mecan & Gestao Ind, P-4200465 Oporto, Portugal. [Turon, Albert] Univ Girona, Dept Engn Mecan & Construccio Ind, Girona, Spain. RP Davila, CG (reprint author), NASA, Langley Res Ctr, Durabil Damage Tolerance & Reliabil Branch, Mail Stop 188E, Hampton, VA 23602 USA. RI Davila, Carlos/D-8559-2011; AMADE Research Group, AMADE/B-6537-2014; Balanzat, Josep Costa/C-1017-2014; Turon, Albert/C-6875-2008; OI AMADE Research Group, AMADE/0000-0002-5778-3291; Turon, Albert/0000-0002-2554-2653; Camanho, Pedro/0000-0003-0363-5207 NR 35 TC 31 Z9 32 U1 4 U2 21 PU AMER INST AERONAUT ASTRONAUT PI RESTON PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA SN 0021-8669 J9 J AIRCRAFT JI J. Aircr. PD MAR-APR PY 2008 VL 45 IS 2 BP 663 EP 672 DI 10.2514/1.32832 PG 10 WC Engineering, Aerospace SC Engineering GA 285FB UT WOS:000254761600034 ER PT J AU Soller, BR Yang, Y Lee, SMC Wilson, C Hagan, RD AF Soller, Babs R. Yang, Ye Lee, Stuart M. C. Wilson, Cassie Hagan, R. Donald TI Noninvasive determination of exercise-induced hydrodgen ion threshold through direct optical measurement SO JOURNAL OF APPLIED PHYSIOLOGY LA English DT Article DE pH; anaerobic threshold; near-infrared spectroscopy; cycling; lactate; carbon dioxide ID NEAR-INFRARED SPECTROSCOPY; SURFACE HISTIDYL RESIDUES; NORMAL ADULT HEMOGLOBIN; VENOUS-BLOOD PH; ANAEROBIC THRESHOLD; GAS-EXCHANGE; REFLECTANCE SPECTROSCOPY; IN-VIVO; SUBMAXIMAL EXERCISE; OXYGEN-SATURATION AB The intensity of exercise above which oxygen uptake (Vo(2)) does not account for all of the required energy to perform work has been associated with lactate accumulation in the blood ( lactate threshold, LT) and elevated carbon dioxide output ( gas exchange threshold). An increase in hydrogen ion concentration ([H+]) is approximately concurrent with elevation of blood lactate and CO2 output during exercise. Near-infrared spectra (NIRS) and invasive interstitial fluid pH (pHm) were measured in the flexor digitorum profundus during handgrip exercise to produce a mathematical model relating the two measures with an estimated error of 0.035 pH units. This NIRS pHm model was subsequently applied to spectra collected from the vastus lateralis of 10 subjects performing an incremental-intensity cycle protocol. Muscle oxygen saturation (SmO2) was also calculated from spectra. We hypothesized that a H (+) threshold could be identified for these subjects and that it would be different from but correlated with the LT. Lactate, gas exchange, SmO2, and H (+) thresholds were determined as a function of Vo(2) using bilinear regression. LT was significantly different from both the gas exchange threshold (Delta = 0.27 +/- 0.29 l/ min) and H+ threshold (Delta = 0.29 +/- 0.23 l/ min), but the gas exchange threshold was not significantly different from the H+ threshold (Delta = 0.00 +/- 0.38 l/min). The H+ threshold was strongly correlated with LT (R-2 = 0.95) and the gas exchange threshold (R-2 = 0.85). This initial study demonstrates the feasibility of noninvasive pHm estimations, the determination of H+ threshold, and the relationship between H+ and classical metabolic thresholds during incremental exercise. C1 [Soller, Babs R.; Yang, Ye] Univ Massachusetts, Sch Med, Dept Anesthesiol, Worcester, MA 01655 USA. [Lee, Stuart M. C.] Wyle Labs, Houston, TX USA. [Wilson, Cassie] JES Tech, Houston, TX USA. [Hagan, R. Donald] NASA, Johnson Space Ctr, Houston, TX USA. RP Soller, BR (reprint author), Univ Massachusetts, Sch Med, Dept Anesthesiol, 55 Lake Ave N, Worcester, MA 01655 USA. EM babs.soller@umassmed.edu NR 43 TC 14 Z9 14 U1 1 U2 10 PU AMER PHYSIOLOGICAL SOC PI BETHESDA PA 9650 ROCKVILLE PIKE, BETHESDA, MD 20814 USA SN 8750-7587 J9 J APPL PHYSIOL JI J. Appl. Physiol. PD MAR PY 2008 VL 104 IS 3 BP 837 EP 844 DI 10.1152/japplphysiol.00849.2007 PG 8 WC Physiology; Sport Sciences SC Physiology; Sport Sciences GA 271XV UT WOS:000253822900035 PM 18096753 ER PT J AU Collins, MW Morris, SB AF Collins, Michael W. Morris, Scott B. TI Testing for adverse impact when sample size is small SO JOURNAL OF APPLIED PSYCHOLOGY LA English DT Article DE selection; adverse impact; significance testing ID 2X2 CONTINGENCY-TABLES; PERSONAL OPINIONS; CONTROVERSY; HOMOGENEITY AB Adverse impact evaluations often call for evidence that the disparity between groups in selection rates is statistically significant, and practitioners must choose which test statistic to apply in this situation. To identify the most effective testing procedure, the authors compared several alternate test statistics in terms of Type I error rates and power, focusing on situations with small samples. Significance testing was found to be of limited value because of low power for all tests. Among the alternate test statistics, the widely-used Z-test on the difference between two proportions performed reasonably well, except when sample size was extremely small. A test suggested by G. J. G. Upton (1982) provided slightly better control of Type I error under some conditions but generally produced results similar to the Z-test. Use of the Fisher Exact Test and Yates's continuity-corrected chi-square test are not recommended because of overly conservative Type I error rates and substantially lower power than the Z-test. C1 [Collins, Michael W.; Morris, Scott B.] IIT, Inst Psychol, Chicago, IL 60616 USA. RP Collins, MW (reprint author), NASA, Lyndon B Johnson Space Ctr, 2101 NASA Pkwy,Mail Code AH, Houston, TX 77058 USA. EM michael.w.collins@nasa.gov NR 20 TC 18 Z9 19 U1 0 U2 15 PU AMER PSYCHOLOGICAL ASSOC PI WASHINGTON PA 750 FIRST ST NE, WASHINGTON, DC 20002-4242 USA SN 0021-9010 J9 J APPL PSYCHOL JI J. Appl. Psychol. PD MAR PY 2008 VL 93 IS 2 BP 463 EP 471 DI 10.1037/0021-9010.93.2.463 PG 9 WC Psychology, Applied; Management SC Psychology; Business & Economics GA 275FJ UT WOS:000254057000018 PM 18361646 ER PT J AU Minnis, P Doelling, DR Nguyen, L Miller, WF Chakrapani, V AF Minnis, Patrick Doelling, David R. Nguyen, Louis Miller, Walter F. Chakrapani, Venkatesan TI Assessment of the visible channel calibrations of the VIRS on TRMM and MODIS on Aqua and Terra SO JOURNAL OF ATMOSPHERIC AND OCEANIC TECHNOLOGY LA English DT Article ID RADIANT ENERGY SYSTEM; IN-FLIGHT CALIBRATION; RADIOMETRIC VALIDATION; PART I; CLOUDS; CERES; INSTRUMENT; SATELLITE; ORBIT; METHODOLOGY AB Several recent research satellites carry self-calibrating multispectral imagers that can be used for calibrating operational imagers lacking complete self-calibrating capabilities. In particular, the visible (VIS, 0.65 mu m) channels on operational meteorological satellites are generally calibrated before launch, but require vicarious calibration techniques to monitor the gains and offsets once they are in orbit. To ensure that the self-calibrating instruments are performing as expected, this paper examines the consistencies between the VIS channel (channel 1) reflectances of the Moderate Resolution Imaging Spectroradiometer (MODIS) instruments on the Terra and Aqua satellites and the version 5a and 6 reflectances of the Visible Infrared Scanner (VIRS) on the Tropical Rainfall Measuring Mission using a variety of techniques. These include comparisons of Terra and Aqua VIS radiances with coincident broadband shortwave radiances from the well-calibrated Clouds and the Earth's Radiant Energy System (CERES), time series of deep convective cloud (DCC) albedos, and ray-matching intercalibrations between each of the three satellites. Time series of matched Terra and VIRS data, Aqua and VIRS data, and DCC reflected fluxes reveal that an older version (version 5a, ending in early 2004) of the VIRS calibration produced a highly stable record, while the latest version (version 6) appears to overestimate the sensor gain change by similar to 1% yr(-1) as the result of a manually induced gain adjustment. Comparisons with the CERES shortwave radiances unearthed a sudden change in the Terra MODIS calibration that caused a 1.17% decrease in the gain on 19 November 2003 that can be easily reversed. After correction for these manual adjustments, the trends in the VIRS and Terra channels are no greater than 0.1% yr(-1). Although the results were more ambiguous, no statistically significant trends were found in the Aqua MODIS channel 1 gain. The Aqua radiances are 1% greater, on average, than their Terra counterparts, and after normalization are 4.6% greater than VIRS radiances, in agreement with theoretical calculations. The discrepancy between the two MODIS instruments should be taken into account to ensure consistency between parameters derived from them. With the adjustments, any of the three instruments can serve as references for calibrating other satellites. Monitoring of the calibrations continues in near-real time and the results are available via the World Wide Web. C1 [Minnis, Patrick; Doelling, David R.; Nguyen, Louis] NASA, Langley Res Ctr, Climate Sci Branch, Hampton, VA 23681 USA. [Miller, Walter F.] Sci Syst & Applicat Inc, Hampton, VA USA. [Chakrapani, Venkatesan] Hampton Univ, Hampton, VA 23668 USA. RP Minnis, P (reprint author), NASA, Langley Res Ctr, Climate Sci Branch, Hampton, VA 23681 USA. EM patrick.minnis-l@nasa.gov RI Minnis, Patrick/G-1902-2010 OI Minnis, Patrick/0000-0002-4733-6148 NR 27 TC 35 Z9 35 U1 0 U2 2 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 0739-0572 J9 J ATMOS OCEAN TECH JI J. Atmos. Ocean. Technol. PD MAR PY 2008 VL 25 IS 3 BP 385 EP 400 DI 10.1175/2007JTECHA1021.1 PG 16 WC Engineering, Ocean; Meteorology & Atmospheric Sciences SC Engineering; Meteorology & Atmospheric Sciences GA 284XL UT WOS:000254741100003 ER PT J AU Lee, JN Hameed, S Shindell, DT AF Lee, Jae N. Hameed, Sultan Shindell, Drew T. TI The northern annular mode in summer and its relation to solar activity variations in the GISS ModelE SO JOURNAL OF ATMOSPHERIC AND SOLAR-TERRESTRIAL PHYSICS LA English DT Article DE stratosphere; troposphere; summer northern annular mode; solar activity ID GREENHOUSE-GAS; SIMULATIONS AB The northern annular mode (NAM) has been successfully used in several studies to understand the variability of the winter atmosphere and its modulation by solar activity. The variability of summer circulation can also be described by the leading empirical orthogonal function (EOF) of geopotential heights. We compare the annular modes of the summer geopotential heights in the northern hemisphere stratosphere and troposphere in the Goddard Institute for Space Studies (GISS) ModelE with those in the National Centers for Environmental Prediction/National Center for Atmospheric Research (NCEP/NCAR) reanalysis. In the stratosphere, the summer NAM obtained from NCEP/NCAR reanalysis as well as from the ModelE simulations has the same sign throughout the northern hemisphere, but shows greater variability at low latitudes. The patterns in both analyses are consistent with the interpretation that low NAM conditions represent an enhancement of the seasonal difference between the summer and the annual averages of geopotential height, temperature and velocity distributions, while the reverse holds for high NAM conditions. Composite analysis of high and low NAM cases in both model and observation suggests that the summer stratosphere is more "summer-like" when the solar activity is near a maximum. This means that the zonal easterly wind flow is stronger and the temperature is higher than normal. Thus increased irradiance favors a low summer NAM. A quantitative comparison of the anti-correlation between the NAM and the solar forcing is presented in the model and in the observation, both of which show lower/higher NAM index in solar maximum/minimum conditions. The temperature fluctuations in simulated solar minimum conditions are greater than in solar maximum throughout the summer stratosphere. The summer NAM in the troposphere obtained from NCEP/NCAR reanalysis has a dipolar zonal structure with maximum variability over the Asian monsoon region. The corresponding EOF in ModelE has a qualitatively similar structure but with less variability in the Asian monsoon region which is displaced eastward of its observed position. In both the NCEP/NCAR reanalysis and the GCM the negative anomalies associated with the NAM in the Euro-Atlantic and Aleutian island regions are enhanced in the solar minimum conditions, though the results are not statistically significant. (C) 2007 Elsevier Ltd. All rights reserved. C1 [Lee, Jae N.; Hameed, Sultan] SUNY Stony Brook, Inst Terr & Planetary Atmospheres, Stony Brook, NY 11794 USA. [Shindell, Drew T.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA. [Shindell, Drew T.] Columbia Univ, New York, NY USA. RP Lee, JN (reprint author), SUNY Stony Brook, Inst Terr & Planetary Atmospheres, Stony Brook, NY 11794 USA. EM jaelee@atmsci.msrc.sunysb.edu RI Shindell, Drew/D-4636-2012 NR 16 TC 4 Z9 6 U1 0 U2 0 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 1364-6826 J9 J ATMOS SOL-TERR PHY JI J. Atmos. Sol.-Terr. Phys. PD MAR PY 2008 VL 70 IS 5 BP 730 EP 741 DI 10.1016/j.jastp.2007.10.012 PG 12 WC Geochemistry & Geophysics; Meteorology & Atmospheric Sciences SC Geochemistry & Geophysics; Meteorology & Atmospheric Sciences GA 285ZP UT WOS:000254815000003 ER PT J AU Iraci, LT Riffel, BG Robinson, CB Michelsen, RR Stephenson, RM AF Iraci, Laura T. Riffel, Brent G. Robinson, Carly B. Michelsen, Rebecca R. Stephenson, Rachel M. TI The acid catalyzed nitration of methanol: formation of methyl nitrate via aerosol chemistry (vol 58, pg 253, 2007) SO JOURNAL OF ATMOSPHERIC CHEMISTRY LA English DT Correction C1 [Iraci, Laura T.; Riffel, Brent G.; Robinson, Carly B.; Michelsen, Rebecca R.; Stephenson, Rachel M.] NASA, Ames Res Ctr, Atmospher Sci Branch, Moffett Field, CA 94035 USA. [Riffel, Brent G.] Univ Calif Davis, Inst Transport Studies, Davis, CA 95616 USA. [Robinson, Carly B.] Univ Colorado, Dept Chem & Biochem, Boulder, CO 80309 USA. [Michelsen, Rebecca R.] Randolph Macon Coll, Dept Chem, Ashland, VA 23005 USA. [Stephenson, Rachel M.] Univ Calif Los Angeles, Dept Chem & Biochem, Los Angeles, CA 90095 USA. RP Iraci, LT (reprint author), NASA, Ames Res Ctr, Atmospher Sci Branch, Mail Stop 245-5, Moffett Field, CA 94035 USA. EM Laura.T.Iraci@NASA.gov NR 1 TC 0 Z9 0 U1 0 U2 2 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0167-7764 J9 J ATMOS CHEM JI J. Atmos. Chem. PD MAR PY 2008 VL 59 IS 3 BP 237 EP 238 DI 10.1007/s10874-008-9098-x PG 2 WC Environmental Sciences; Meteorology & Atmospheric Sciences SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences GA 332MS UT WOS:000258087700006 ER PT J AU Lin, JL Lee, MI Kim, D Kang, IS Frierson, DMW AF Lin, Jia-Lin Lee, Myong-In Kim, Daehyun Kang, In-Sik Frierson, Dargan M. W. TI The impacts of convective parameterization and moisture triggering on AGCM-simulated convectively coupled equatorial waves SO JOURNAL OF CLIMATE LA English DT Article ID MADDEN-JULIAN OSCILLATION; GENERAL-CIRCULATION MODEL; TROPICAL INTRASEASONAL OSCILLATIONS; SIMPLE MULTICLOUD PARAMETERIZATION; AIR-SEA INTERACTION; PART I; LOW-FREQUENCY; KELVIN WAVES; STRATIFORM INSTABILITY; CUMULUS CONVECTION AB This study examines the impacts of convective parameterization and moisture convective trigger on convectively coupled equatorial waves simulated by the Seoul National University (SNU) atmospheric general circulation model (AGCM). Three different convection schemes are used, including the simplified Arakawa-Schubert (SAS) scheme, the Kuo (1974) scheme, and the moist convective adjustment (MCA) scheme, and a moisture convective trigger with variable strength is added to each scheme. The authors also conduct a "no convection" experiment with deep convection schemes turned off. Space-time spectral analysis is used to obtain the variance and phase speed of dominant convectively coupled equatorial waves, including the Madden-Julian oscillation (MJO), Kelvin, equatorial Rossby (ER), mixed Rossby-gravity (MRG), and eastward inertio-gravity (EIG) and westward inertio-gravity (WIG) waves. The results show that both convective parameterization and the moisture convective trigger have significant impacts on AGCM-simulated, convectively coupled equatorial waves. The MCA scheme generally produces larger variances of convectively coupled equatorial waves including the MJO, more coherent eastward propagation of the MJO, and a more prominent MJO spectral peak than the Kuo and SAS schemes. Increasing the strength of the moisture trigger significantly enhances the variances and slows down the phase speeds of all wave modes except the MJO, and usually improves the eastward propagation of the MJO for the Kuo and SAS schemes, but the effect for the MCA scheme is small. The no convection experiment always produces one of the best signals of convectively coupled equatorial waves and the MJO. C1 [Lin, Jia-Lin] CIRES Climate Diagnost Ctr, Boulder, CO USA. [Lin, Jia-Lin] NOAA, Earth Syst Res Lab, Boulder, CO USA. [Lee, Myong-In] NASA, GSFC, Global Modeling & Assimilat Off, Greenbelt, MD USA. [Kim, Daehyun; Kang, In-Sik] Seoul Natl Univ, Sch Earth & Environm Sci, Seoul, South Korea. [Frierson, Dargan M. W.] Univ Chicago, Dept Geophys Sci, Chicago, IL 60637 USA. RP Lin, JL (reprint author), Ohio State Univ, Dept Geog, Columbus, OH 43210 USA. EM lin789@osu.edu RI Frierson, Dargan/F-1763-2010; 안, 민섭/D-9972-2015; OI Frierson, Dargan/0000-0001-8952-5644; Lee, Myong-In/0000-0001-8983-8624 NR 94 TC 69 Z9 69 U1 0 U2 6 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 0894-8755 J9 J CLIMATE JI J. Clim. PD MAR PY 2008 VL 21 IS 5 BP 883 EP 909 DI 10.1175/2007JCLI1790.1 PG 27 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 278DK UT WOS:000254263700003 ER PT J AU Schoeberl, MR Douglass, AR Newman, PA Lait, LR Lary, D Waters, J Livesey, N Froidevaux, L Lambert, A Read, W Filipiak, MJ Pumphrey, HC AF Schoeberl, M. R. Douglass, A. R. Newman, P. A. Lait, L. R. Lary, D. Waters, J. Livesey, N. Froidevaux, L. Lambert, A. Read, W. Filipiak, M. J. Pumphrey, H. C. TI QBO and annual cycle variations in tropical lower stratosphere trace gases from HALOE and Aura MLS observations SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID QUASI-BIENNIAL OSCILLATION; WATER-VAPOR; OCCULTATION EXPERIMENT; EOS MLS; OZONE; SATELLITE; CIRCULATION; TROPOSPHERE; ATMOSPHERE; TRANSPORT AB We have analyzed thirteen years ( 1993 to 2005) of HALOE and over two years of EOS MLS observations ( September 2004 to December 2006) for QBO and annual cycle trace variations in tropical H2O, HCl, ozone, N2O, CO, HF, and CH4. We use these results to develop the theory explaining both Brewer-Dobson circulation (BDC) and QBO driven fluctuations in tropical trace gases. For H2O, BDC variations drive part of the tropopause annual forcing through annual variations in the temperature as has been shown previously. For CO, the annual variations in the BDC amplify the annual fluctuations in CO at the tropopause as has recently been shown by Randel et al (2007). In both cases, the tropopause signal is carried upward by the mean BDC. For ozone, N2O, HCl and other gases, photochemical processes force fluctuations in the trace gases to be synchronized with annual and QBO variations in the zonal mean residual vertical velocity as is shown using lag correlations. C1 [Schoeberl, M. R.; Douglass, A. R.; Newman, P. A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Lait, L. R.; Lary, D.] Univ Maryland Baltimore Cty, Baltimore, MD 21228 USA. [Waters, J.; Livesey, N.; Froidevaux, L.; Lambert, A.; Read, W.] NASA, Jet Propuls Lab, Pasadena, CA USA. [Filipiak, M. J.; Pumphrey, H. C.] Univ Edinburgh, Sch Geosci, Edinburgh, Midlothian, Scotland. RP Schoeberl, MR (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. EM schom@zephyr.gsfc.nasa.gov RI Lary, David/A-6163-2010; Newman, Paul/D-6208-2012; Douglass, Anne/D-4655-2012 OI Newman, Paul/0000-0003-1139-2508; NR 39 TC 46 Z9 46 U1 0 U2 4 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 MAR 1 PY 2008 VL 113 IS D5 AR D05301 DI 10.1029/2007JD008678 PG 15 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 270JB UT WOS:000253716000001 ER PT J AU Wang, PKC Hadaegh, FY AF Wang, P. K. C. Hadaegh, F. Y. TI Stability analysis of switched dynamical systems with state-space dilation and contraction SO JOURNAL OF GUIDANCE CONTROL AND DYNAMICS LA English DT Article; Proceedings Paper CT AIAA Guidance, Navigation, and Control Conference CY AUG 21-24, 2006 CL Keystone, CO ID MULTIPLE LYAPUNOV FUNCTIONS AB This paper considers switched dynamical systems with state-space dilation and contraction formed by concatenating the states of a set of local dynamical systems or semiflows on state spaces with different dimensions at specified time instants. These systems arise naturally in many aerospace applications, such as multibody dynamic systems involving changes in the degrees of freedom and systems composed of multiple spacecraft with docking and undocking capabilities flying information. The notions of stability of invariant sets in the sense of Lyapunov for usual dynamical systems are extended to this class of switched dynamical systems. Also, the notion of finite-time stability with specified bounds is introduced. Sufficient stability conditions are established for a special class of switched dynamical systems with state-space dilation and contraction. Their application to spacecraft formation stability analysis is discussed. C1 [Wang, P. K. C.] Univ Calif Los Angeles, Dept Elect Engn, Los Angeles, CA 90095 USA. [Hadaegh, F. Y.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Wang, PKC (reprint author), Univ Calif Los Angeles, Dept Elect Engn, Los Angeles, CA 90095 USA. NR 14 TC 10 Z9 11 U1 0 U2 0 PU AMER INST AERONAUT ASTRONAUT PI RESTON PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA SN 0731-5090 J9 J GUID CONTROL DYNAM JI J. Guid. Control Dyn. PD MAR-APR PY 2008 VL 31 IS 2 BP 395 EP 401 DI 10.2514/1.28407 PG 7 WC Engineering, Aerospace; Instruments & Instrumentation SC Engineering; Instruments & Instrumentation GA 272RF UT WOS:000253876600012 ER PT J AU Hughes, SP AF Hughes, Steven P. TI General method for optimal guidance of spacecraft formations SO JOURNAL OF GUIDANCE CONTROL AND DYNAMICS LA English DT Article ID RELATIVE MOTION; ELLIPTIC ORBITS; DESIGN; LISA AB One of the most interesting and challenging aspects of formation guidance algorithm design is the coupling of the orbit design and the science return. The effectiveness of the formation as a science instrument is intimately coupled with the relative geometry and evolution of the collection of spacecraft. Therefore, the science return can be maximized by optimizing the orbit design according to a performance metric relevant to the science mission goals. In this work, we present a general method for optimal formation guidance that is applicable to missions whose performance metric, requirements, and constraints can be cast as functions that are explicitly dependent upon the orbit states and spacecraft relative positions and velocities. The approach is fully nonlinear, accommodates orbital perturbations, and is applicable to multiple flight regimes including highly eccentric, hyperbolic, interplanetary, or libration point orbits. Furthermore, the method is applicable to small formations, as well as large formations and constellations. We present a general form for the cost and constraint functions, and derive their semi-analytic gradients with respect to the formation initial conditions. The gradients are broken down into two types. The first type are gradients of the mission-specific performance metric with respect to formation geometry. The second type are derivatives of the formation geometry with respect to the orbit initial conditions. The fact that these two types of derivatives appear separately allows us to derive and implement a general framework that requires minimal modification to be applied to different missions or mission phases. To illustrate the applicability of the approach, we conclude with applications to two missions: the Magnetospheric Multiscale Mission, and the Laser Interferometer Space Antenna. C1 NASA, Goddard Space Flight Ctr, Flight Dynam Anal Branch, Greenbelt, MD 20771 USA. RP Hughes, SP (reprint author), NASA, Goddard Space Flight Ctr, Flight Dynam Anal Branch, Greenbelt, MD 20771 USA. RI NASA MMS, Science Team/J-5393-2013 OI NASA MMS, Science Team/0000-0002-9504-5214 NR 32 TC 10 Z9 11 U1 0 U2 8 PU AMER INST AERONAUT ASTRONAUT PI RESTON PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA SN 0731-5090 J9 J GUID CONTROL DYNAM JI J. Guid. Control Dyn. PD MAR-APR PY 2008 VL 31 IS 2 BP 414 EP 423 DI 10.2514/1.23731 PG 10 WC Engineering, Aerospace; Instruments & Instrumentation SC Engineering; Instruments & Instrumentation GA 272RF UT WOS:000253876600014 ER PT J AU Markley, FL AF Markley, F. Landis TI Unit quaternion from rotation matrix SO JOURNAL OF GUIDANCE CONTROL AND DYNAMICS LA English DT Article ID DIRECTION-COSINE MATRIX; SINGULARITY-FREE EXTRACTION; VECTOR OBSERVATIONS C1 NASA, Goddard Space Flight Ctr, Guidance Navigat & Control Syst Engn Branch, Greenbelt, MD 20771 USA. RP Markley, FL (reprint author), NASA, Goddard Space Flight Ctr, Guidance Navigat & Control Syst Engn Branch, Code 591, Greenbelt, MD 20771 USA. NR 17 TC 5 Z9 6 U1 0 U2 4 PU AMER INST AERONAUT ASTRONAUT PI RESTON PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA SN 0731-5090 J9 J GUID CONTROL DYNAM JI J. Guid. Control Dyn. PD MAR-APR PY 2008 VL 31 IS 2 BP 440 EP 442 DI 10.2514/1.31730 PG 3 WC Engineering, Aerospace; Instruments & Instrumentation SC Engineering; Instruments & Instrumentation GA 272RF UT WOS:000253876600019 ER PT J AU Mehta, SK Tyring, SK Gilden, DH Cohrs, RJ Leal, MJ Castro, VA Feiveson, AH Ott, CM Pierson, DL AF Mehta, Satish K. Tyring, Stephen K. Gilden, Donald H. Cohrs, Randall J. Leal, Melanie J. Castro, Victoria A. Feiveson, Alan H. Ott, C. Mark Pierson, Duane L. TI Varicella-zoster virus in the saliva of patients with herpes zoster SO JOURNAL OF INFECTIOUS DISEASES LA English DT Article; Proceedings Paper CT 32nd International Herpesvirus Workshop CY JUL 07-12, 2007 CL Asheville, NC ID SINE HERPETE; REACTIVATION; INFECTION AB Fifty-four patients with herpes zoster were treated with valacyclovir. On treatment days 1, 8, and 15, pain was scored and saliva examined for varicella-zoster virus (VZV) DNA. VZV DNA was found in every patient the day treatment was started and later disappeared in 82%. There was a positive correlation between the presence of VZV DNA and pain and between VZV DNA copy number and pain (P<.0005). VZV DNA was present in 1 patient before rash and in 4 after pain resolved and was not present in any of 6 subjects with chronic pain or in 14 healthy subjects. Analysis of human saliva has potential usefulness in the diagnosis of neurological disease produced by VZV without rash. C1 [Gilden, Donald H.; Cohrs, Randall J.] Univ Colorado, Hlth Sci Ctr, Dept Neurol, Denver, CO 80262 USA. [Gilden, Donald H.] Univ Colorado, Hlth Sci Ctr, Dept Microbiol, Denver, CO 80262 USA. [Tyring, Stephen K.] Univ Texas Houston, Hlth Sci Ctr, Houston, TX USA. [Feiveson, Alan H.; Ott, C. Mark; Pierson, Duane L.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. [Mehta, Satish K.; Leal, Melanie J.; Castro, Victoria A.] Enterprise Advisory Serv Inc, Houston, TX USA. RP Gilden, DH (reprint author), Univ Colorado, Hlth Sci Ctr, Dept Neurol, Mail Stop B-182,4200 E 9th Ave, Denver, CO 80262 USA. EM don.gilden@uchsc.edu FU NIA NIH HHS [AG06127, R01 AG006127, R01 AG006127-20, R37 AG006127]; NINDS NIH HHS [NS32623, P01 NS032623, P01 NS032623-20] NR 15 TC 41 Z9 43 U1 0 U2 3 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0022-1899 J9 J INFECT DIS JI J. Infect. Dis. PD MAR 1 PY 2008 VL 197 IS 5 BP 654 EP 657 DI 10.1086/527420 PG 4 WC Immunology; Infectious Diseases; Microbiology SC Immunology; Infectious Diseases; Microbiology GA 271FD UT WOS:000253773400006 PM 18260763 ER PT J AU Tahmasebi, F AF Tahmasebi, Farhad TI Closure to "Discussion of 'Kinematics of a new high-precision three-degree-of-freedom parallel manipulator" (2008, ASME J. Mech. Des., 130, p. 035501) SO JOURNAL OF MECHANICAL DESIGN LA English DT Editorial Material ID MINIMANIPULATOR C1 NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Tahmasebi, F (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. EM farhad.tahmasebi@nasa.gov NR 14 TC 0 Z9 0 U1 0 U2 0 PU ASME-AMER SOC MECHANICAL ENG PI NEW YORK PA THREE PARK AVE, NEW YORK, NY 10016-5990 USA SN 1050-0472 J9 J MECH DESIGN JI J. Mech. Des. PD MAR PY 2008 VL 130 IS 3 AR 035502 PG 2 WC Engineering, Mechanical SC Engineering GA 276MA UT WOS:000254144900017 ER PT J AU Robichaud, DJ Hodges, JT Brown, LR Lisak, D Maslowski, P Yeung, LY Okumura, M Miller, CE AF Robichaud, David J. Hodges, Joseph T. Brown, Linda R. Lisak, Daniel Maslowski, Piotr Yeung, Laurence Y. Okumura, Mitchio Miller, Charles E. TI Experimental intensity and lineshape parameters of the oxygen A-band using frequency-stabilized cavity ring-down spectroscopy SO JOURNAL OF MOLECULAR SPECTROSCOPY LA English DT Article DE oxygen; A-band; intensities; cavity ring-down spectroscopy ID FOURIER-TRANSFORM SPECTROSCOPY; MOLECULAR LINE ABSORPTION; SCATTERING ATMOSPHERE; QUANTITATIVE MEASUREMENTS; LASER SPECTROSCOPY; PRESSURE-SHIFT; HIGH-PRECISION; BROADENED HF; O-2; TRANSITIONS AB Line intensities, self- and air-broadened linewidths, pressure-induced shifts, and collisional narrowing coefficients were measured from 2 <= J'<= 32 in the P branch of the O-2 A-band (12975-13110 cm(-1)) utilizing Galatry line profiles. Spectra were recorded using the frequency-stabilized cavity ring-down spectrometer located at NIST, Gaithersburg, MD with a spectral resolution <0.0001 cm(-1) and noise-equivalent absorption coefficient of 6 x 10(-8) m(-1) Hz(-1/2). Line intensities, obtained from calibrated gas samples for 2 <= X <= 32, are similar to 1% lower than the values in current spectroscopic databases. At higher J(18 <= J' <= 32), the measured air- and self- broadened half widths are up to 20% lower than the extrapolated values given in HITRAN 2004, while corresponding half-widths for 2 <= J' <= 15 are in better agreement. Available self-broadened half widths are fitted to empirical expressions with an rms of 0.8%. We discuss the implications of our results for accurate remote sensing of surface pressure and photon path length distributions. (C) 2008 Published by Elsevier Inc. C1 [Hodges, Joseph T.; Lisak, Daniel; Maslowski, Piotr] NIST, Proc Measurments Div, Gaithersburg, MD 20899 USA. [Robichaud, David J.; Yeung, Laurence Y.; Okumura, Mitchio] CALTECH, Div Chem & Chem Engn, Pasadena, CA 91125 USA. [Brown, Linda R.; Miller, Charles E.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Lisak, Daniel; Maslowski, Piotr] Uniwersytet Mikolaja Kopernika, Inst Fizyki, PL-87100 Torun, Poland. RP Hodges, JT (reprint author), NIST, Proc Measurments Div, 100 Bureau Dr, Gaithersburg, MD 20899 USA. EM joseph.bodges@nist.gov; Linda.R.Brown@jpl.nasa.gov; mo@caltech.edu; charles.e.miller@jpl.nasa.gov RI Hodges, Joseph/B-4578-2009; Yeung, Laurence/D-4574-2009; Lisak, Daniel/E-1470-2014; Maslowski, Piotr/H-4476-2014; Okumura, Mitchio/I-3326-2013 OI Yeung, Laurence/0000-0001-9901-2607; Maslowski, Piotr/0000-0001-8882-7106; Okumura, Mitchio/0000-0001-6874-1137 NR 61 TC 49 Z9 48 U1 1 U2 17 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0022-2852 EI 1096-083X J9 J MOL SPECTROSC JI J. Mol. Spectrosc. PD MAR PY 2008 VL 248 IS 1 BP 1 EP 13 DI 10.1016/j.jms.2007.10.010 PG 13 WC Physics, Atomic, Molecular & Chemical; Spectroscopy SC Physics; Spectroscopy GA 264BI UT WOS:000253259800001 ER PT J AU Thadathil, P Thoppil, P Rao, RR Muraleedharan, PM Somayajulu, YK Gopalakrishna, VV Murtugudde, R Reddy, GV Revichandran, C AF Thadathil, Pankajakshan Thoppil, Prasad Rao, R. R. Muraleedharan, P. M. Somayajulu, Y. K. Gopalakrishna, V. V. Murtugudde, Raghu Reddy, G. V. Revichandran, C. TI Seasonal variability of the observed barrier layer in the Arabian sea SO JOURNAL OF PHYSICAL OCEANOGRAPHY LA English DT Article ID NORTH INDIAN-OCEAN; EQUATORIAL PACIFIC-OCEAN; SURFACE-LAYER; MIXED-LAYER; TOGA DECADE; DYNAMICS; MONSOON; SALINITY; MODEL; THERMODYNAMICS AB The formation mechanisms of the barrier layer ( BL) and its seasonal variability in the Arabian Sea ( AS) are studied using a comprehensive dataset of temperature and salinity profiles from Argo and other archives for the AS. Relatively thick BL of 20-60 m with large spatial extent is found in the central-southwestern AS ( CSWAS), the convergence zone of the monsoon wind, during the peak summer monsoon ( July-August) and in the southeastern AS ( SEAS) and northeastern AS ( NEAS) during the winter ( January-February). Although the BL in the SEAS has been reported before, the observed thick BL in the central-southwestern AS during the peak summer monsoon and in the northeastern AS during late winter are the new findings of this study. The seasonal variability of BL thickness ( BLT) is closely related to the processes that occur during summer and winter monsoons. During both seasons, the Ekman processes and the distribution of low-salinity waters in the surface layer show a dominant influence on the observed BLT distributions. In addition, Kelvin and Rossby waves also modulate the observed BL thickness in the AS. The relatively low salinity surface water overlying the Arabian Sea high-salinity water ( ASHSW) provides an ideal ground for strong haline stratification in the CSWAS ( during summer monsoon) and in NEAS ( during winter monsoon). During summer, northward advection of equatorial low-salinity water by the Somali Current and the offshore advection of low-salinity water from the upwelling region facilitate the salinity stratification that is necessary to develop the observed BL in the CSWAS. In the SEAS, during winter, the winter monsoon current ( WMC) carries less saline water over relatively high salinity ambient water to form the observed BL there. The winter West India Coastal Current ( WICC) transports the low-salinity water from the SEAS to the NEAS, where it lies over the subducted ASHSW leading to strong haline stratification. Ekman pumping together with the downwelling Kelvin wave in the NEAS deepen the thermocline to cause the observed thick BL in the NEAS. C1 [Thadathil, Pankajakshan; Muraleedharan, P. M.; Somayajulu, Y. K.; Gopalakrishna, V. V.; Reddy, G. V.] Natl Inst Oceanog, Panaji, Goa, India. [Thoppil, Prasad] Univ So Mississippi, Dept Marine Sci, Hattiesburg, MS 39406 USA. [Thoppil, Prasad] NASA, Stenis Space Ctr, Mississippi State, MS USA. [Rao, R. R.] Naval Phys Oceanog Lab, Kochi, India. [Murtugudde, Raghu] Univ Maryland, Earth Sci Interdisciplinary Ctr, College Pk, MD 20742 USA. [Revichandran, C.] Natl Inst Oceanog, Reg Ctr, Kochi, India. RP Thadathil, P (reprint author), Natl Inst Oceanog, Panaji, Goa, India. EM pankaj@nio.org NR 53 TC 15 Z9 15 U1 0 U2 3 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 0022-3670 J9 J PHYS OCEANOGR JI J. Phys. Oceanogr. PD MAR PY 2008 VL 38 IS 3 BP 624 EP 638 DI 10.1175/2007JPO3798.1 PG 15 WC Oceanography SC Oceanography GA 276EQ UT WOS:000254124500005 ER PT J AU Walsh, EJ Banner, ML Wright, CW Vandemark, DC Chapron, B Jensen, J Lee, S AF Walsh, E. J. Banner, M. L. Wright, C. W. Vandemark, D. C. Chapron, B. Jensen, J. Lee, S. TI The southern ocean waves experiment. Part III: Sea surface slope statistics and near-nadir remote sensing SO JOURNAL OF PHYSICAL OCEANOGRAPHY LA English DT Article ID PROBABILITY DENSITY-FUNCTIONS; SPECTRUM SPATIAL VARIATION; WIND-GENERATED WAVES; ATMOSPHERIC STABILITY; RADAR BACKSCATTER; MODEL; DEPENDENCE; SCATTERING AB During the Southern Ocean Waves Experiment (SOWEX), registered ocean wave topography and backscattered power data at Ka band ( 36 GHz) were collected with the NASA Scanning Radar Altimeter ( SRA) off the coast of Tasmania under a wide range of wind and sea conditions, from quiescent to gale-force winds with 9-m significant wave height. Collection altitude varied from 35 m to over 1 km, allowing determination of the sea surface mean square slope ( mss), the directional wave spectrum, and the detailed variation of backscattered power with incidence angle, which deviated from a simple Gaussian scattering model. The non-Gaussian characteristics of the backscatter increased systematically with the mss, suggesting that a global model to characterize Ka-band radar backscatter from the sea surface within 25 of nadir might be possible. C1 [Walsh, E. J.; Wright, C. W.] NASA, Goddard Space Flight Ctr, Wallops Isl, VA USA. [Banner, M. L.] Univ New S Wales, Sch Math, Sydney, NSW, Australia. [Vandemark, D. C.] Univ New Hampshire, Ocean Proc Anal Lab, Durham, NH 03824 USA. [Chapron, B.] IFREMER, Ctr Brest, Dept Oceanog Spatiale, F-29280 Plouzane, France. [Jensen, J.] Natl Ctr Atmospher Res, Res Aircraft Facil, Broomfield, CO USA. [Lee, S.] CSIRO Marine & Atmospher Res, Aspendale, Vic, Australia. RP Walsh, EJ (reprint author), NOAA, Earth Syst Res Lab, PSD3 325 Broadway, Boulder, CO 80305 USA. EM edward.walsh@nasa.gov RI Jensen, Jorgen/C-9211-2009; Chapron, Bertrand/O-6527-2015; OI Banner, Michael/0000-0002-0799-5341 NR 31 TC 11 Z9 11 U1 1 U2 7 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 0022-3670 EI 1520-0485 J9 J PHYS OCEANOGR JI J. Phys. Oceanogr. PD MAR PY 2008 VL 38 IS 3 BP 670 EP 685 DI 10.1175/2007JPO3771.1 PG 16 WC Oceanography SC Oceanography GA 276EQ UT WOS:000254124500008 ER PT J AU Whitacre, JF Zaghib, K West, WC Ratnakumar, BV AF Whitacre, J. F. Zaghib, K. West, W. C. Ratnakumar, B. V. TI Dual active material composite cathode structures for Li-ion batteries SO JOURNAL OF POWER SOURCES LA English DT Article DE mixed active material cathodes; Li battery; LiFePO4; LiNiMnO2; LiCoO2; hybrid ID X-RAY-DIFFRACTION; ELECTROCHEMICAL-BEHAVIOR; LAYERED CATHODE; PERFORMANCE; ELECTRODES; CAPACITY; HYBRID; SPINEL; CELLS; LIMN2O4 AB The efficacy of composite Li-ion battery cathodes made by mixing active materials that possessed either high-rate capability or high specific energy was examined. The cathode structures studied contained carbon-coated LiFePO4 and either Li[Li0.17Mn0.58Ni0.25]O-2 or LiCoO2. These active materials were arranged using three different electrode geometries: fully intermixed, fully separated, or layered. Discharge rate studies, cycle-life evaluation, and electrochemical impedance spectroscopy studies were conducted using coin cell test structures containing Li-metal anodes. Results indicated that electrode configuration was correlated to rate capability and degree of polarization if there was a large differential between the rate capabilities of the two active material species. (C) 2007 Elsevier B.V. All rights reserved. C1 [Whitacre, J. F.] Carnegie Mellon Univ, Dept Mat Sci & Engn, Pittsburgh, PA 15213 USA. [Whitacre, J. F.] Carnegie Mellon Univ, Dept Engn & Publ Policy, Pittsburgh, PA 15213 USA. [Zaghib, K.] Inst Rech Hydro Quebec, Varennes, PQ J3X 1S1, Canada. [West, W. C.; Ratnakumar, B. V.] CALTECH, Jet Prop Lab, Electrochem Technol Grp, Pasadena, CA 91109 USA. RP Whitacre, JF (reprint author), Carnegie Mellon Univ, Dept Mat Sci & Engn, Pittsburgh, PA 15213 USA. EM whitacre@andrew.cmu.edu NR 31 TC 34 Z9 37 U1 2 U2 54 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0378-7753 J9 J POWER SOURCES JI J. Power Sources PD MAR 1 PY 2008 VL 177 IS 2 BP 528 EP 536 DI 10.1016/j.jpowsour.2007.11.076 PG 9 WC Chemistry, Physical; Electrochemistry; Energy & Fuels; Materials Science, Multidisciplinary SC Chemistry; Electrochemistry; Energy & Fuels; Materials Science GA 272QE UT WOS:000253873700035 ER PT J AU Alahmad, M Hess, H Mojarradi, M West, W Whitacre, J AF Alahmad, Mahmoud Hess, Herb Mojarradi, Mohammad West, William Whitacre, Jay TI Battery switch array system with application for JPL's rechargeable micro-scale batteries SO JOURNAL OF POWER SOURCES LA English DT Article DE battery; battery scheduling; battery system; microbattery; power management; reconfigurable architecture AB A battery switch array system is developed for solid-state rechargeable micro-scale lithium batteries, designed and developed by Jet Propulsion Laboratory (JPL), California Institute of Technology, for aerospace applications. The heart of the system is a topology unique in its dynamic reconfiguration ability by providing selective connection and isolation and versatile in its core design by incorporating passive, active or energy storage elements. It allows up to N-batteries to be connected in any desired configuration; providing maximum voltage, maximum capacity and a voltage/capacity ratio. This battery switch array system is part of a power management system that is developed to utilize these features and provide for multiple charging algorithms, real time status information and fault tolerant capabilities. A two microbattery prototype circuit is built using a microprocessor-based controller for verification of the system design and its features. The topology and its features will be explored in this paper to provide methods for modular and scalable energy storage system design. (C) 2007 Elsevier B.V. All rights reserved. C1 [Alahmad, Mahmoud; Hess, Herb] Univ Idaho, Moscow, ID 83843 USA. [Mojarradi, Mohammad; West, William; Whitacre, Jay] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Alahmad, M (reprint author), Univ Idaho, Moscow, ID 83843 USA. EM malahmad2@unl.edu; hhess@ece.uidaho.edu; Mohammad.M.Mojarradi@JPL.NASA.GOV; W.C.West@JPL.NASA.GOV; J.F.Whitacre@JPL.NASA.GOV NR 19 TC 12 Z9 12 U1 0 U2 7 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0378-7753 J9 J POWER SOURCES JI J. Power Sources PD MAR 1 PY 2008 VL 177 IS 2 BP 566 EP 578 DI 10.1016/j.jpowsour.2007.11.053 PG 13 WC Chemistry, Physical; Electrochemistry; Energy & Fuels; Materials Science, Multidisciplinary SC Chemistry; Electrochemistry; Energy & Fuels; Materials Science GA 272QE UT WOS:000253873700040 ER PT J AU Mulenburg, G AF Mulenburg, Gerald TI Rainbows & ratholes: Best practices for managing successful projects SO JOURNAL OF PRODUCT INNOVATION MANAGEMENT LA English DT Book Review C1 [Mulenburg, Gerald] NASA, Washington, DC 20546 USA. NR 2 TC 0 Z9 0 U1 0 U2 0 PU BLACKWELL PUBLISHING PI OXFORD PA 9600 GARSINGTON RD, OXFORD OX4 2DQ, OXON, ENGLAND SN 0737-6782 J9 J PROD INNOVAT MANAG JI J. Prod. Innov. Manage. PD MAR PY 2008 VL 25 IS 2 BP 207 EP 209 DI 10.1111/j.1540-5885.2008.00294_3.x PG 3 WC Business; Engineering, Industrial; Management SC Business & Economics; Engineering GA 268LZ UT WOS:000253582600010 ER PT J AU Titov, E Gallagher-Rogers, A Levin, D Reed, B AF Titov, E. Gallagher-Rogers, A. Levin, D. Reed, Brian TI Examination of a collision-limiter direct simulation Monte Carlo method for micropropulsion applications SO JOURNAL OF PROPULSION AND POWER LA English DT Article ID FLOW; NOZZLES AB A wide range of flow regimes occur in micronozzles, from the transitional to the continuum regime, which prevents the use of a single computational method such as direct simulation Monte Carlo or computational fluid dynamics and Navier-Stokes. A collision-limiter approach is proposed that extends the applicability of direct simulation Monte Carlo to the continuum regime and can be used to solve a wide range of microelectromechanical system flows when it is coupled with the baseline direct simulation Monte Carlo. A comparison of the results obtained with this computational technique with new experimental data and Navier-Stokes results suggests consistency between experimental and computational methods for three-dimensional microelectromechanical system micronozzles with stagnation pressures on the order of 5 atm. However, the level of agreement was found to vary with the nozzle geometry, suggesting that additional research is needed for both computations and experiments in this flow regime. C1 [Titov, E.; Gallagher-Rogers, A.; Levin, D.] Penn State Univ, Dept Aerosp Engn, University Pk, PA 16802 USA. [Reed, Brian] NASA, John H Glenn Res Ctr Lewis Field, Elect Propuls Branch, Cleveland, OH 44135 USA. RP Titov, E (reprint author), Penn State Univ, Dept Aerosp Engn, University Pk, PA 16802 USA. NR 27 TC 8 Z9 8 U1 0 U2 3 PU AMER INST AERONAUT ASTRONAUT PI RESTON PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA SN 0748-4658 J9 J PROPUL POWER JI J. Propul. Power PD MAR-APR PY 2008 VL 24 IS 2 BP 311 EP 321 DI 10.2514/1.28793 PG 11 WC Engineering, Aerospace SC Engineering GA 274QW UT WOS:000254016900018 ER PT J AU Leonard, C Diehr, M Rosmus, P Maguire, WC AF Leonard, C. Diehr, M. Rosmus, P. Maguire, W. C. TI Radiative transition probabilities in the X-2 Pi(g) state of CO2+ SO JOURNAL OF QUANTITATIVE SPECTROSCOPY & RADIATIVE TRANSFER LA English DT Article DE carbon dioxide; carbon dioxide cation; dipole moment function; Renner-Teller effect; rovibronic intensities; radiative; transition probabilities; thermal emission spectrum; Mars' atmosphere ID ULTRAVIOLET SPECTROMETER EXPERIMENT; THERMAL EMISSION SPECTROMETER; TRIATOMIC-MOLECULES; VARIATIONAL METHOD; VIBRONIC STRUCTURE; UPPER ATMOSPHERE; ENERGY-LEVELS; MARS; BANDS; ION AB Using ab initio calculated potential energy and electric dipole moment functions, absolute radiative transition probabilities between the rovibronic Renner-Teller states of the electronic ground state X-2 Pi(g) of CO2+ have been evaluated. The rovibronic eigenstates were obtained (up to 6500 cm(-1) and J <= 13/2) from variational calculations including the Renner-Teller and spin-orbit angular momentum couplings. The absolute intensities for the rovibrational states of the neutral CO2 electronic ground state, calculated by a similar approach, are found to be in excellent agreement with experimental data. For CO2+ the presented results are expected to have similar accuracy. It is found that the overtone intensities of the antisymmetric stretching mode of CO2+ are of similar magnitude as the fundamental transitions, in contrast with CO2. The theoretically generated IR-emission spectrum is compared with the limb spectrum of the Mars atmosphere, measured by the Thermal Emission Spectrometer on Mars Global Surveyor. (C) 2007 Elsevier Ltd. All rights reserved. C1 [Leonard, C.; Diehr, M.; Rosmus, P.] Univ Marne la Vallee, Chim Theor Lab, Marne La Vallee 2, France. [Maguire, W. C.] NASA, Goddard Space Flight Ctr, Solar Syst Explorat Div, Greenbelt, MD 20771 USA. RP Leonard, C (reprint author), Univ Marne la Vallee, Chim Theor Lab, EA 2180,5 Blvd Descartes,Champs Marne 77454, Marne La Vallee 2, France. EM celine.leonard@univ-mlv.fr OI LEONARD, Celine/0000-0003-0303-3505 NR 55 TC 8 Z9 8 U1 0 U2 6 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0022-4073 J9 J QUANT SPECTROSC RA JI J. Quant. Spectrosc. Radiat. Transf. PD MAR PY 2008 VL 109 IS 4 BP 535 EP 548 DI 10.1016/j.jqsrt.2007.07.011 PG 14 WC Optics; Spectroscopy SC Optics; Spectroscopy GA 242JD UT WOS:000251720500001 ER PT J AU Lattanzi, V Walters, A Pearson, JC Drouin, BJ AF Lattanzi, Valerio Walters, Adam Pearson, John C. Drouin, Brian J. TI THz spectrum of monodeuterated methane SO JOURNAL OF QUANTITATIVE SPECTROSCOPY & RADIATIVE TRANSFER LA English DT Article DE methane; line positions; deuterated methane; interstellar spectra ID ELECTRIC DIPOLE MOMENT; OUTER SOLAR-SYSTEM; D/H ISOTOPIC RATIO; GROUND-STATE; ROTATIONAL SPECTRUM; CH3D; ABUNDANCE; SPECTROSCOPY; DEUTERIUM; TITAN AB We report new measurements of the rotational spectrum of monodeuterated methane (CH3D) in the range of 690-1200 GHz which allow for an accurate prediction of all lines in the range of the high-resolution spectrometer of the Herschel Space Observatory. Comparison is also made with the previous analysis based on infrared combination differences. Three lines of (CH3D)-C-13 were measured in natural abundance. (C) 2007 Elsevier Ltd. All rights reserved. C1 [Pearson, John C.; Drouin, Brian J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Lattanzi, Valerio; Walters, Adam] Ctr Etud Spatiale Rayonnements, F-31028 Toulouse 4, France. [Lattanzi, Valerio] Univ Roma La Sapienza, Dept Phys, Rome, Italy. RP Drouin, BJ (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM brian.j.drouin@jpl.nasa.gov NR 38 TC 11 Z9 11 U1 0 U2 10 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0022-4073 J9 J QUANT SPECTROSC RA JI J. Quant. Spectrosc. Radiat. Transf. PD MAR PY 2008 VL 109 IS 4 BP 580 EP 586 DI 10.1016/j.jqsrt.2007.09.002 PG 7 WC Optics; Spectroscopy SC Optics; Spectroscopy GA 242JD UT WOS:000251720500005 ER PT J AU Reda, DC Wilder, MC Bogdanoff, DW Prabhu, DK AF Reda, D. C. Wilder, M. C. Bogdanoff, D. W. Prabhu, D. K. TI Transition experiments on blunt bodies with distributed roughness in hypersonic free flight SO JOURNAL OF SPACECRAFT AND ROCKETS LA English DT Article; Proceedings Paper CT AIAA 45th Aerospace Sciences Meeting and Exhibit CY JAN 08-11, 2007 CL Reno, NV SP Amer Inst Aeronaut & Astronaut ID BOUNDARY-LAYER-TRANSITION AB Models of hemispherical and blunt large-angle conical geometries were flown in the NASA Ames hypersonic ballistic range to investigate the influence of distributed surface roughness on transition to turbulence. Transition-zone fronts were defined from optically measured global surface temperature distributions. Measurements of preconditioned surface roughness, surface temperature, average transition-front location, and freestream environment were combined with real-gas Navier-Stokes calculations of model flowfields, including laminar boundary-layer development in these flowfields, to transform all data into dimensionless parameters used to correlate transition onset/location on rough blunt bodies in hypersonic flow. A combination of present and previously published results led to the formulation of a transition correlation applicable over all three regimes potentially encountered by an ablating blunt-body heat shield undergoing atmospheric entry: the smooth-wall asymptote, the critical-roughness Reynolds number regime, and the large-roughness/low-Reynolds-number asymptote. C1 [Reda, D. C.] NASA, Ames Res Ctr, Space Technol Div, Moffett Field, CA 94035 USA. [Bogdanoff, D. W.; Prabhu, D. K.] ELORET Corp, Sunnyvale, CA 94086 USA. [Wilder, M. C.] NASA, Ames Res Ctr, Reacting Flow Environm Branch, Moffett Field, CA 94035 USA. RP Reda, DC (reprint author), NASA, Ames Res Ctr, Space Technol Div, Mail Stop 229-3, Moffett Field, CA 94035 USA. NR 12 TC 5 Z9 5 U1 2 U2 6 PU AMER INST AERONAUT ASTRONAUT PI RESTON PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA SN 0022-4650 J9 J SPACECRAFT ROCKETS JI J. Spacecr. Rockets PD MAR-APR PY 2008 VL 45 IS 2 BP 210 EP 215 DI 10.2514/1.30288 PG 6 WC Engineering, Aerospace SC Engineering GA 285FE UT WOS:000254761900006 ER PT J AU Berry, SA Horvath, TJ AF Berry, Scott A. Horvath, Thomas J. TI Discrete-roughness transition for hypersonic flight vehicles SO JOURNAL OF SPACECRAFT AND ROCKETS LA English DT Article; Proceedings Paper CT AIAA 45th Aerospace Sciences Meeting and Exhibit CY JAN 08-11, 2007 CL Reno, NV SP Amer Inst Aeronaut & Astronaut ID SHUTTLE ORBITER; TUNNEL AB The importance of discrete roughness and the correlations developed to predict the onset of boundary-layer transition on hypersonic flight vehicles are discussed. The paper is organized by hypersonic vehicle applications characterized in a general sense by the boundary layer: slender with hypersonic conditions at the edge of the boundary layer, moderately blunt with supersonic, and blunt with subsonic. This paper is intended to be a review of recent discrete-roughness-transition work completed at NASA Langley Research Center in support of agency flight test programs. First, a review is provided of discrete-roughness wind-tunnel data and the resulting correlations that were developed. Then results obtained from flight vehicles (in particular, the recently flown Hyper-X and shuttle missions) are discussed and compared with the ground-based correlations. Based on these comparisons, wind-tunnel-derived roughness criteria are shown to provide a reliable means for predicting transition behavior for flight vehicles. C1 [Berry, Scott A.; Horvath, Thomas J.] NASA, Langley Res Ctr, Aerothermodynam Branch, Res & Technol Directorate, Hampton, VA 23681 USA. RP Berry, SA (reprint author), NASA, Langley Res Ctr, Aerothermodynam Branch, Res & Technol Directorate, Mail Stop 408A, Hampton, VA 23681 USA. NR 49 TC 15 Z9 16 U1 2 U2 6 PU AMER INST AERONAUT ASTRONAUT PI RESTON PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA SN 0022-4650 J9 J SPACECRAFT ROCKETS JI J. Spacecr. Rockets PD MAR-APR PY 2008 VL 45 IS 2 BP 216 EP 227 DI 10.2514/1.30970 PG 12 WC Engineering, Aerospace SC Engineering GA 285FE UT WOS:000254761900007 ER PT J AU Covington, MA Heinemann, JM Goldstein, HE Chen, YK Terrazas-Salinas, I Balboni, JA Olejniczak, J Martinez, ER AF Covington, M. A. Heinemann, J. M. Goldstein, H. E. Chen, Y. -K. Terrazas-Salinas, I. Balboni, J. A. Olejniczak, J. Martinez, E. R. TI Performance of a low density ablative heat shield material SO JOURNAL OF SPACECRAFT AND ROCKETS LA English DT Article; Proceedings Paper CT AIAA 37th Thermophysics Conference CY JUN 28-JUL 01, 2004 CL Portland, OR SP AIAA AB An evaluation of the Stardust spacecraft forebody heat shield design was conducted to address uncertainties in original development and qualification efforts. Results are reported for additional arc jet tests and analyses done on the ablative and thermal performance of the low density ablative material used in the Stardust design for conditions simulating nominal peak convective heating conditions expected for Stardust sample return capsule Earth entry. Test data were used to adjust iteratively the thermophysical properties in an ablative response computer code to match experimental in-depth temperatures. Ablative recession rates and maximum internal temperatures were satisfactorily predicted by the computer code using derived properties for nominal peak entry heating rates and for rates 37% greater than nominal. Experimental and computer model maximum internal material temperatures were in agreement over a range of conditions and are considered to validate the Stardust heat shield design although measured in-depth temperature data show consistent temperature rise deviations that are not accurately modeled by the computer code. Predicted Stardust heat shield performance based on these results indicates that maximum attachment bond line temperatures will be considerably less than the maximum allowable of 250 degrees C, and total recession will be a small fraction of the as-designed thickness. C1 [Goldstein, H. E.] NASA, Ames Res Ctr, Adv Comp Sci Res Inst, Moffett Field, CA 94035 USA. [Covington, M. A.; Heinemann, J. M.] Eloret Corp, Sunnyvale, CA 94086 USA. NR 14 TC 9 Z9 12 U1 1 U2 9 PU AMER INST AERONAUT ASTRONAUT PI RESTON PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA SN 0022-4650 J9 J SPACECRAFT ROCKETS JI J. Spacecr. Rockets PD MAR-APR PY 2008 VL 45 IS 2 BP 237 EP 247 DI 10.2514/1.12403 PG 11 WC Engineering, Aerospace SC Engineering GA 285FE UT WOS:000254761900009 ER PT J AU Grebow, DJ Ozimek, MT Howell, KC Folta, DC AF Grebow, Daniel J. Ozimek, Martin T. Howell, Kathleen C. Folta, David C. TI Multibody orbit architectures for lunar south pole coverage SO JOURNAL OF SPACECRAFT AND ROCKETS LA English DT Article; Proceedings Paper CT AAS/AIAA 16th Space Flight Mechanics Meeting CY JAN 22-26, 2006 CL Tampa, FL SP Amer Astronaut Soc, Amer Inst Aeronaut & Astronaut ID 3-DIMENSIONAL PERIODIC-ORBITS; TRAJECTORY DESIGN; HALO ORBITS; POINT; CONSTELLATIONS AB A potential ground station at the lunar south pole has prompted studies of orbit architectures that ensure adequate coverage. The creation of multibody orbit constellations begins with an investigation of periodic orbits in the circular restricted three-body problem. A detailed analysis of halo and vertical families, as well as other orbits near the libration points in the vicinity of the moon, suggests that constant communications can be achieved with two spacecraft in combinations of Earth-moon libration-point orbits. In particular, the investigation focuses on nine different orbits from these families with periods ranging from 7 to 16 days. Natural solutions are generated in a full-ephemeris model including solar perturbations. Possible ground stations on the moon and the Earth are established for coverage results and verification of communications capabilities. Preliminary station-keeping costs are also computed for long-term communications with the ground stations. C1 [Grebow, Daniel J.; Ozimek, Martin T.; Howell, Kathleen C.] Purdue Univ, Sch Aeronaut & Astronaut, W Lafayette, IN 47907 USA. [Folta, David C.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Grebow, DJ (reprint author), Purdue Univ, Sch Aeronaut & Astronaut, Armstrong Hall,701 W Stadium Ave, W Lafayette, IN 47907 USA. NR 32 TC 16 Z9 16 U1 0 U2 3 PU AMER INST AERONAUT ASTRONAUT PI RESTON PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA SN 0022-4650 J9 J SPACECRAFT ROCKETS JI J. Spacecr. Rockets PD MAR-APR PY 2008 VL 45 IS 2 BP 344 EP 358 DI 10.2514/1.28738 PG 15 WC Engineering, Aerospace SC Engineering GA 285FE UT WOS:000254761900020 ER PT J AU Wilson, JL Mazzoleni, AP DeJarnette, FR Antol, J Hajos, GA Strickland, CV AF Wilson, Jamie L. Mazzoleni, Andre P. DeJarnette, Fred R. Antol, Jeffrey Hajos, Gregory A. Strickland, Christopher V. TI Design, analysis, and testing of Mars Tumbleweed rover concepts SO JOURNAL OF SPACECRAFT AND ROCKETS LA English DT Article ID DYNAMICS; PLANE; BALL; MOTION; BODY AB A Mars Tumbleweed rover is a spherical, wind-driven, planetary rover. Compared with conventional rovers, a tumbleweed rover can travel farther faster and gain access to areas such as valleys and chasms that previously were inaccessible. This paper presents design, mathematical modeling, computer simulation, and testing of various tumbleweed rover concepts. In particular, we present wind-tunnel data indicating that a box-kite configuration represents a promising tumbleweed rover design, we show that a working box-kite-type tumbleweed can be constructed, and we show that center of mass variation shows promise as the basis of a tumbleweed rover navigation system. C1 [Wilson, Jamie L.] N Carolina State Univ, Raleigh, NC 27695 USA. [Antol, Jeffrey; Hajos, Gregory A.] NASA, Langley Res Ctr, Architectures Missions & Sci Branch, Hampton, VA 23681 USA. [Strickland, Christopher V.] NASA, Wallops Flight Facil, Mech Syst Branch, Wallops Isl, VA 23337 USA. NR 46 TC 12 Z9 15 U1 0 U2 9 PU AMER INST AERONAUTICS ASTRONAUTICS PI RESTON PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA SN 0022-4650 EI 1533-6794 J9 J SPACECRAFT ROCKETS JI J. Spacecr. Rockets PD MAR-APR PY 2008 VL 45 IS 2 BP 370 EP 382 DI 10.2514/1.31288 PG 13 WC Engineering, Aerospace SC Engineering GA 285FE UT WOS:000254761900022 ER PT J AU Britch, SC Linthicum, KJ Anyamba, A Tucker, CJ Pak, EW AF Britch, Seth C. Linthicum, Kenneth J. Anyamba, Assaf Tucker, Compton J. Pak, Edwin W. CA Mosquito Surveillance Team TI Long-term surveillance data and patterns of invasion by Aedes albopictus in Florida SO JOURNAL OF THE AMERICAN MOSQUITO CONTROL ASSOCIATION LA English DT Article DE Aedes albopictus; Florida; geographic information system (GIS); mosquito-borne virus; normalized difference vegetation index (NDVI) ID UNITED-STATES; AEGYPTI; AFRICA; SPREAD; VECTOR; COUNTY; FIELD AB We used geographic information system (GIS) and long-term mosquito surveillance data from Lake, Pasco, Manatee, and Sarasota Counties, FL, to look at patterns of invasion by Aedes albopictus and concurrent changes in resident Ae. aegypti. We investigated environmental factors associated with population changes in these species with the use of satellite climate data. Aedes aegypti densities attenuated rapidly following the arrival of Ae. albopictus in most counties, yet both species persisted in equilibrium in Manatee County. We discuss the relative importance of rainfall, habitat, and proximity to urban areas in the population dynamics of these species in sympatry. C1 [Britch, Seth C.; Linthicum, Kenneth J.] USDA ARS, Ctr Med Agr & Vet Entomol, Gainesville, FL 32608 USA. [Anyamba, Assaf; Tucker, Compton J.; Pak, Edwin W.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Mosquito Surveillance Team] Manatee Cty Mosquito Control Dist, Palmetto, FL 34220 USA. [Mosquito Surveillance Team] Lake Cty Mosquito & Aquat Plant Management, Tavares, FL 32778 USA. [Mosquito Surveillance Team] Pasco Cty Mosquito Control Dist, Odessa, FL 33556 USA. [Mosquito Surveillance Team] Sarasota Cty Mosquito Control Dist, Sarasota, FL 34233 USA. RP Britch, SC (reprint author), USDA ARS, Ctr Med Agr & Vet Entomol, 1600-1700 SW 23rd Dr, Gainesville, FL 32608 USA. RI Valle, Ruben/A-7512-2013 NR 17 TC 15 Z9 16 U1 2 U2 11 PU AMER MOSQUITO CONTROL ASSOC PI EATONTOWN PA P O BOX 234, EATONTOWN, NJ 07724-0234 USA SN 8756-971X J9 J AM MOSQUITO CONTR JI J. Am. Mosq. Control Assoc. PD MAR PY 2008 VL 24 IS 1 BP 115 EP 120 DI 10.2987/5594.1 PG 6 WC Entomology SC Entomology GA 280FH UT WOS:000254410300020 PM 18437824 ER PT J AU Tesfaye, S Rowan, MG Mueller, K Trudgill, BD Harding, DJ AF Tesfaye, S. Rowan, M. G. Mueller, K. Trudgill, B. D. Harding, D. J. TI Relay and accommodation zones in the Dobe and Hanle grabens, central Afar, Ethiopia and Djibouti SO JOURNAL OF THE GEOLOGICAL SOCIETY LA English DT Article ID NORMAL-FAULT SYSTEMS; AFRICAN RIFT SYSTEM; HYDROCARBON EXPLORATION; SEGMENT LINKAGE; BLOCK ROTATION; EAST-AFRICA; RAMPS; DISPLACEMENT; EXTENSION; GEOMETRY AB The right-stepping Dobe and Hanle grabens display a variety of structures that serve to transfer extensional displacement. These structures range from relay zones between overlapping fault segments to accommodation zones between interacting rift segments. The study reveals the presence of three examples of displacement transfer structures: a breached relay zone, a large-scale accommodation zone that is partially breached, and a composite zone that combines elements of both. All three examples exhibit common structural elements. First, dipping ramps develop between horizontal horst blocks and graben floors. Second, these ramps are cut by numerous faults, most of which are antithetic to the ramps and the graben boundary faults. The antithetic faults bound elongate blocks that are rotated into the grabens. Third, crosscutting faults partially or completely link the en echelon or overlapping graben boundary faults. The identification of precursory structures (mode I fractures) at the leading edge of the Dobe-Hanle accommodation zone breaching faults suggest that the breaching process may be continuing. The spatial alignment from north to south of the crosscutting faults, open fractures and lineaments indicates that the breaching process is progressing from the Dobe graben towards the Hanle graben. C1 [Tesfaye, S.] Lincoln Univ, Cooperat Res Program, Jefferson City, MO 65102 USA. [Rowan, M. G.] Rowan Consulting Inc, Boulder, CO 80302 USA. [Mueller, K.] Univ Colorado, Dept Geol Sci, Boulder, CO 80309 USA. [Trudgill, B. D.] Colorado Sch Mines, Dept Geol & Geol Engn, Golden, CO 80401 USA. [Harding, D. J.] NASA, Goddard Space Flight Ctr, Planetary Geodynam Lab, Greenbelt, MD 20771 USA. RP Tesfaye, S (reprint author), Lincoln Univ, Cooperat Res Program, 104 Foster Hall,820 Chestnut St, Jefferson City, MO 65102 USA. EM tesfayes@lincolnu.edu NR 49 TC 7 Z9 7 U1 2 U2 9 PU GEOLOGICAL SOC PUBL HOUSE PI BATH PA UNIT 7, BRASSMILL ENTERPRISE CENTRE, BRASSMILL LANE, BATH BA1 3JN, AVON, ENGLAND SN 0016-7649 J9 J GEOL SOC LONDON JI J. Geol. Soc. PD MAR PY 2008 VL 165 BP 535 EP 547 DI 10.1144/0016-76492007-093 PN 2 PG 13 WC Geosciences, Multidisciplinary SC Geology GA 272RC UT WOS:000253876200008 ER PT J AU Ramon, ML Nelson, PA De Martini, E Walsh, WJ Bernardi, G AF Ramon, Marina L. Nelson, Peter A. De Martini, Edward Walsh, William J. Bernardi, Giacomo TI Phylogeography, historical demography, and the role of post-settlement ecology in two Hawaiian damselfish species SO MARINE BIOLOGY LA English DT Article ID PELAGIC LARVAL DURATION; CORAL-REEF FISH; GREAT-BARRIER-REEF; DASCYLLUS-ALBISELLA; MARINE POPULATIONS; GENETIC-STRUCTURE; SPATIAL-PATTERNS; DISPERSAL; MITOCHONDRIAL; CONNECTIVITY AB Coral reef fish generally have relatively sedentary juvenile and adult phases and a presumed highly dispersive pelagic larval phase, yet previous studies that have tried to relate pelagic larval duration (PLD) to population structure have given inconsistent results. In the present study, the population structures of two damselfishes, Stegastes fasciolatus and Dascyllus albisella, were examined using mitochondrial control region sequences. The two species have similar PLDs (similar to 25 and 27 days respectively), but consistently differ in their settlement preferences, habitat, and densities in populations throughout the Hawaiian Archipelago, from Hawaii north to Kure Atoll, and south to Johnston Atoll. Information on habitat preferences and population densities were collected between September 2000 and October 2002, and tissue samples for the genetic studies were collected between January and April 2004. Based on the differences in habitat and abundance of the two species, the expectation was that S. fasciolatus would have high genetic variability but little population structure compared to D. albisella, and this was largely confirmed. Stegastes fasciolatus had little population structure in most of the Hawaiian Islands, and D. albisella showed evidence of strong population structure throughout its range. An exception to this pattern was the large difference between the Kure Atoll population of S. fasciolatus and all others. These results suggest that the interaction of several biological factors (e.g. species-specific spawning habitat and season) with environmental factors (e.g. seasonal wind and current patterns) may have more influence on population structure than single life history characteristics, such as the PLD. C1 [Ramon, Marina L.; Nelson, Peter A.] Univ Calif Santa Cruz, Dept Ecol & Evolut Biol, Santa Cruz, CA 95060 USA. [Nelson, Peter A.] HT Harvey & Associates, Los Gatos, CA 95032 USA. [De Martini, Edward] SW Fisheries Sci Ctr, Natl Marine Fisheries Serv, Ntal Ocean & Atmospher Adm, Honolulu, HI 96822 USA. [Walsh, William J.] Div Aquat Resources, Kailua, HI 96740 USA. RP Bernardi, G (reprint author), Univ Calif Santa Cruz, Dept Ecol & Evolut Biol, 100 Shaffer Rd, Santa Cruz, CA 95060 USA. EM bernardi@biology.ucsc.edu RI Bernardi, Giacomo/F-6346-2011 OI Bernardi, Giacomo/0000-0002-8249-4678 NR 61 TC 20 Z9 20 U1 1 U2 11 PU SPRINGER HEIDELBERG PI HEIDELBERG PA TIERGARTENSTRASSE 17, D-69121 HEIDELBERG, GERMANY SN 0025-3162 EI 1432-1793 J9 MAR BIOL JI Mar. Biol. PD MAR PY 2008 VL 153 IS 6 BP 1207 EP 1217 DI 10.1007/s00227-007-0894-7 PG 11 WC Marine & Freshwater Biology SC Marine & Freshwater Biology GA 265HZ UT WOS:000253351000019 ER PT J AU Roth, DJ Seebo, JP Winfree, WP AF Roth, Don J. Seebo, Jeffrey P. Winfree, William P. TI Simultaneous Noncontact Precision Imaging of Microstructural and Thickness Variation in Dielectric Materials Using Terahertz Energy SO MATERIALS EVALUATION LA English DT Article DE space shuttle; external tank; thermal protection system; sprayon foam insulation; terahertz; velocity; thickness; density ID ULTRASONIC VELOCITY AB This paper describes a noncontact, single-sided terahertz electromagnetic measurement and imaging technique that simultaneously characterizes microstructural (for example, spatially lateral density) and thickness variation in dielectric (insulating) materials. The technique was demonstrated for two materials - space shuttle external tank spray-on foam insulation and a silicon nitride ceramic. It is believed that this technique can be used for current and future NASA thermal protection systems and other dielectric material testing applications, where microstructural and thickness variation require precision mapping. Scaling up to more complex shapes, such as cylindrical structures and structures with beveled regions, would appear to be feasible. C1 [Roth, Don J.] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. [Seebo, Jeffrey P.] NASA, Langley Res Ctr, Lockheed Martin Space Syst Co, Hampton, VA 23681 USA. RP Roth, DJ (reprint author), NASA, Glenn Res Ctr, 21000 Brookpk Rd, Cleveland, OH 44135 USA. EM donald.j.roth@nasa.gov NR 26 TC 4 Z9 4 U1 0 U2 1 PU AMER SOC NONDESTRUCTIVE TEST PI COLUMBUS PA 1711 ARLINGATE LANE PO BOX 28518, COLUMBUS, OH 43228-0518 USA SN 0025-5327 J9 MATER EVAL JI Mater. Eval. PD MAR PY 2008 VL 66 IS 3 BP 325 EP 331 PG 7 WC Materials Science, Characterization & Testing SC Materials Science GA 373NJ UT WOS:000260978400004 ER PT J AU Connolly, HC Smith, C Benedix, G Folco, L Righter, K Zipfel, J Yamaguchi, A Aoudjehane, HC AF Connolly, Harold C., Jr. Smith, Caroline Benedix, Gretchen Folco, Luigi Righter, Kevin Zipfel, Jutta Yamaguchi, Akira Aoudjehane, Hasnaa Chennaoui TI The Meteoritical Bulletin, No. 93, 2008 March SO METEORITICS & PLANETARY SCIENCE LA English DT Article AB In this edition of the Meteoritical Bulletin, 1443 approved meteorite names with their relevant data are reported, one from a specific location within Africa, 2 11 from Northwest Africa, 5 from KOR-EAMET, 598 from the Chinese Antarctic Expedition, 23 from the Americas, 151 from Asia, three from Australia, two from Europe, two from NOVA, and 447 from ANSMET that were not reported in the Meteoritical Bulletin no. 87. Also reported are 4 falls frorn the Americas. Sonic highlights of approved meteorites are 10 lunar (including NWA 5000, an 11.528 kg sample), 3 Martian, 4 irons (one from Indonesia), 2 ureilites, 5 mesosiderites, I pallasite, 6 brachinites, 3 CV3s, 4 CO3s, 8 CMs, 12 CK3s, and many more. Finally, the Committee on Nomenclature of the Meteoritical Society announces two new names series in North America. C1 [Connolly, Harold C., Jr.] CUNY, Dept Phys Sci, Kingsborough Community Coll, Brooklyn, NY 11235 USA. [Connolly, Harold C., Jr.] CUNY, Grad Sch, Brooklyn, NY 11235 USA. [Connolly, Harold C., Jr.] Amer Museum Nat Hist, Dept Earth & Planetary Sci, New York, NY 10024 USA. [Connolly, Harold C., Jr.] Univ Arizona, Lunar & Planetary Lab, Dept Planetary Sci, Tucson, AZ 85721 USA. [Smith, Caroline; Benedix, Gretchen] Nat Hist Museum, Dept Mineral, London SW7 5BD, England. [Folco, Luigi] Museo Nazl Antartide, I-53100 Siena, Italy. [Righter, Kevin] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. [Zipfel, Jutta] Forsch Inst, Sekt Meteoritenforsch, D-60325 Frankfurt, Germany. [Zipfel, Jutta] Nat Museum Senckenberg, D-60325 Frankfurt, Germany. [Yamaguchi, Akira] Natl Inst Polar Res, Antarctic Meteorite Res Ctr, Tokyo 1738515, Japan. [Aoudjehane, Hasnaa Chennaoui] Univ Hassan II Casablanca, Fac Sci, Dept Geol, Casablanca, Morocco. RP Connolly, HC (reprint author), CUNY, Dept Phys Sci, Kingsborough Community Coll, 2001 Oriental Blvd, Brooklyn, NY 11235 USA. EM meteorite@kingsborough.edu OI Benedix, Gretchen/0000-0003-0990-8878 NR 3 TC 23 Z9 23 U1 3 U2 5 PU METEORITICAL SOC PI FAYETTEVILLE PA DEPT CHEMISTRY/BIOCHEMISTRY, UNIV ARKANSAS, FAYETTEVILLE, AR 72701 USA SN 1086-9379 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD MAR PY 2008 VL 43 IS 3 BP 571 EP 632 PG 62 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 339GQ UT WOS:000258566500010 ER PT J AU Leeuw, TK Tsyboulski, DA Nikolaev, PN Bachilo, SM Arepalli, S Weisman, RB AF Leeuw, Tonya K. Tsyboulski, Dmitri A. Nikolaev, Pavel N. Bachilo, Sergei M. Arepalli, Sivaram Weisman, R. Bruce TI Strain measurements on individual single-walled carbon nanotubes in a polymer host: Structure-dependent spectral shifts and load transfer SO NANO LETTERS LA English DT Article ID COMPOSITES; PHOTOLUMINESCENCE; FLUORESCENCE; STRENGTH AB The fluorescence spectra of individual semiconducting single-walled carbon nanotubes embedded in polymer films were measured during the application of controlled stretching and compressive strains. Nanotube band gaps were found to shift in systematic patterns that depend on the (n,m) structural type and are in excellent agreement with the predictions of theoretical models. Loss of nanotube - host adhesion was revealed by abrupt irregularities in plots of spectral shift vs strain. C1 [Leeuw, Tonya K.; Tsyboulski, Dmitri A.; Bachilo, Sergei M.; Weisman, R. Bruce] Rice Univ, Dept Chem, Richard E Smalley Inst Nanoscale Sci & Technol, Houston, TX 77005 USA. [Leeuw, Tonya K.; Tsyboulski, Dmitri A.; Bachilo, Sergei M.; Weisman, R. Bruce] Rice Univ, Ctr Biol Environm Nanotechnol, Houston, TX 77005 USA. [Nikolaev, Pavel N.; Arepalli, Sivaram] NASA, Lyndon B Johnson Space Ctr, ERC Inc, Houston, TX 77058 USA. RP Weisman, RB (reprint author), Rice Univ, Dept Chem, Richard E Smalley Inst Nanoscale Sci & Technol, 6100 Main St, Houston, TX 77005 USA. EM weisman@rice.edu RI Arepalli, Sivaram/A-5372-2010; OI Weisman, R. Bruce/0000-0001-8546-9980 NR 28 TC 39 Z9 39 U1 8 U2 23 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 MAR PY 2008 VL 8 IS 3 BP 826 EP 831 DI 10.1021/nl072861c 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 273QS UT WOS:000253947400011 PM 18298093 ER PT J AU Wolff, JA Ramos, FC Hart, GL Patterson, JD Brandon, AD AF Wolff, J. A. Ramos, F. C. Hart, G. L. Patterson, J. D. Brandon, A. D. TI Columbia River flood basalts from a centralized crustal magmatic system SO NATURE GEOSCIENCE LA English DT Article ID LARGE IGNEOUS PROVINCES; OS ISOTOPE SYSTEMATICS; YELLOWSTONE HOTSPOT; PACIFIC-NORTHWEST; PLUME HEAD; MANTLE; ORIGIN; CONTAMINATION; VOLCANISM; PLATEAU AB The Columbia River Basalt Group in the northwestern United States(1), comprising about 230,000 cubic kilometres of rock, exhibits unusual patterns in lava distribution, geochemistry and its apparent relationship to regional tectonics. Consequently, there is little consensus on the origin of its magmas(2-12). Here, we examine the isotopic ratios of Sr, Nd, Pb and Os and trace-element abundances in Columbia River basalts. The results suggest that most of the lava was produced when magma derived from a mantle plume assimilated continental crust in a central magma chamber system located at the boundary between the North American craton and the accreted terranes of Idaho and Oregon. Other, related basalts are the product of mixing between the mantle plume and different types of regional upper mantle. Magma was then transported over a wide region by an extensive network of dykes, a process that has been identified in other flood basalt provinces as well(13). Interactions of the plume with surrounding upper mantle, and of mantle-derived magmas with regional crust, provide a relatively simple(6,7,9,14,15) model to explain the more unusual features of the main-phase Columbia River Basalts. C1 [Wolff, J. A.; Hart, G. L.] Washington State Univ, Sch Earth & Environm Sci, Pullman, WA 99164 USA. [Ramos, F. C.; Patterson, J. D.] Cent Washington Univ, Dept Geol Sci, Ellensburg, WA 98926 USA. [Brandon, A. D.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. RP Wolff, JA (reprint author), Washington State Univ, Sch Earth & Environm Sci, Pullman, WA 99164 USA. EM jawolff@mail.wsu.edu NR 30 TC 41 Z9 41 U1 2 U2 23 PU NATURE PUBLISHING GROUP PI NEW YORK PA 75 VARICK ST, 9TH FLR, NEW YORK, NY 10013-1917 USA SN 1752-0894 J9 NAT GEOSCI JI Nat. Geosci. PD MAR PY 2008 VL 1 IS 3 BP 177 EP 180 DI 10.1038/ngeo124 PG 4 WC Geosciences, Multidisciplinary SC Geology GA 309AZ UT WOS:000256433400016 ER PT J AU Sullivan, BM Davies, P Hodgdon, KK Salamone, JA Pilon, A AF Sullivan, Brenda M. Davies, Patricia Hodgdon, Kathleen K. Salamone, Joseph A. Pilon, Anthony TI Realism assessment of sonic boom simulators SO NOISE CONTROL ENGINEERING JOURNAL LA English DT Article ID LOUDNESS; NOISE AB Developments in small supersonic aircraft design are predicted to result in low-intensity sonic booms. Booms generated by current aircraft are similar to those that led to the ban on commercial supersonic flight over the US, so are unsuitable for parametric studies of psychoacoustic response to low-intensity booms. Therefore, simulators have been used to study the impact of predicted low-intensity sonic booms. However, simulators have been criticized because, when simulating conventional-level booms, the sounds were observed to be unrealistic by people experienced in listening to sonic booms. Thus, two studies were conducted to measure the perceived realism of three sonic boom simulators. Experienced listeners rated the realism of conventional sonic boom signatures when played in these simulators. The effects on perceived realism of factors such as duration of post-boom noise, exclusion of very low frequency components, inclusion of ground reflections, and type of simulator were examined. Duration of post-boom noise was found to have a strong effect on perceived realism, while type of simulator had a weak effect. It was determined that post-boom noise had to be at least 1.5 seconds long for the sound to be rated very realistic. Loudness level did not affect realism for the range of sounds played in the tests (80-93 dB ASEL). (C) 2008 Institute of Noise Control Engineering. C1 [Sullivan, Brenda M.] NASA, Langley Res Ctr, Struct Acoust Branch, Hampton, VA 23681 USA. [Davies, Patricia] Purdue Univ, Sch Mech Engn, Ray W Herrick Labs, W Lafayette, IN 47907 USA. [Hodgdon, Kathleen K.] Penn State Univ, Appl Res Lab, State Coll, PA 16801 USA. [Salamone, Joseph A.] Gulfstream Aerosp Corp, Savannah, GA 31407 USA. [Pilon, Anthony] Lockheed Martin Aeronaut Co, Adv Dev Programs, Palmdale, CA 93599 USA. RP Sullivan, BM (reprint author), NASA, Langley Res Ctr, Struct Acoust Branch, Mail Stop 463, Hampton, VA 23681 USA. EM brenda.m.suillivan@nasa.gov; daviesp@ecn.purdue.edu; kkh2@psu.edu; joe.salamone@gulfstream.com; tony.pilon@lmco.com NR 25 TC 2 Z9 2 U1 0 U2 0 PU INST NOISE CONTROL ENGINEERING PI AMES PA IOWA STATE UNIV, COLLEGE ENGINEERING, 212 MARSTON HALL, AMES, IA 50011-2152 USA SN 0736-2501 J9 NOISE CONTROL ENG J JI Noise Control Eng. J. PD MAR-APR PY 2008 VL 56 IS 2 BP 141 EP 157 DI 10.3397/1.2919547 PG 17 WC Acoustics; Engineering, Multidisciplinary SC Acoustics; Engineering GA 309KT UT WOS:000256460000005 ER PT J AU Mariani, F Orsini, S Candidi, M Marcucci, MF Acuna, M Musmann, G Ness, NF AF Mariani, F. Orsini, S. Candidi, M. Marcucci, M. F. Acuna, M. Musmann, G. Ness, N. F. TI On the current circulation about a high-voltage s/c: Two more case-studies by the TSS-1R tethered satellite mission SO NUOVO CIMENTO DELLA SOCIETA ITALIANA DI FISICA C-GEOPHYSICS AND SPACE PHYSICS LA English DT Article ID FIELD AB Magnetic field observations by the TEMAG experiment on the TSS-1R satellite for two events of constant stimulated current along the tether are discussed. Previous evidence of a complex, unexpected, electric azimuthal current circulation in close proximity of the high-voltage spacecraft is further supported and complemented. While previous events cover time intervals shorter than a spill cycle, the two new ones allow a complete coverage for a full spin cycle. The reed of deeper theoretical approach as well as of more experimental observations is stressed. C1 [Mariani, F.] Univ Roma Tor Vergata, Dipartimento Fis, Rome, Italy. [Orsini, S.; Candidi, M.; Marcucci, M. F.] INAF CNR, Ist Fis Spazio Interplanetario, Rome, Italy. [Acuna, M.] NASA, GSFC, Greenbelt, MD 20771 USA. [Musmann, G.] Tech Univ Carolo Wilhelmina Braunschweig, Braunschweig, Germany. [Ness, N. F.] Univ Delaware, Newark, DE USA. RP Mariani, F (reprint author), Univ Roma Tor Vergata, Dipartimento Fis, Rome, Italy. EM franco.mariani@roma2.infn.it NR 5 TC 1 Z9 1 U1 0 U2 0 PU SOC ITALIANA FISICA PI BOLOGNA PA VIA SARAGOZZA, 12, I-40123 BOLOGNA, ITALY SN 1124-1896 J9 NUOVO CIMENTO C JI Nuovo Cimento Soc. Ital. Fis. C-Geophys. Space Phys. PD MAR-APR PY 2008 VL 31 IS 2 BP 135 EP 141 DI 10.1393/ncc/i2008-10287-3 PG 7 GA 393PZ UT WOS:000262386500002 ER PT J AU Lagerloef, G Colomb, FR Le Vine, D Wentz, F Yueh, S Ruf, C Lilly, J Gunn, J Chao, Y deCharon, A Feldman, G Swift, C AF Lagerloef, Gary Colomb, F. Raul Le Vine, David Wentz, Frank Yueh, Simon Ruf, Christopher Lilly, Jonathan Gunn, John Chao, Yi deCharon, Annette Feldman, Gene Swift, Calvin TI THE AQUARIUS/SAC-D MISSION: DESIGNED TO MEET THE SALINITY REMOTE-SENSING CHALLENGE SO OCEANOGRAPHY LA English DT Article ID SEA-SURFACE SALINITY; L-BAND; OCEAN SALINITY; SMOS MISSION; SPACE; RETRIEVAL; MODEL C1 [Lagerloef, Gary] NASA, Aquarius Miss Earth & Space Res, Seattle, WA USA. [Colomb, F. Raul] CONAE, Argentine Space Agcy, Buenos Aires, DF, Argentina. [Le Vine, David] NASA, Goddard Space Flight Ctr, Instrument Sci Branch, NASA Aquarius Miss, Greenbelt, MD 20771 USA. [Wentz, Frank] Remote Sensing Syst, Santa Rosa, CA USA. [Yueh, Simon; Chao, Yi] NASA, Jet Prop Lab, Pasadena, CA USA. [Ruf, Christopher] Univ Michigan, Space Phys Res Lab, Ann Arbor, MI 48109 USA. [Lilly, Jonathan; Gunn, John] Earth & Space Res, Seattle, WA USA. [deCharon, Annette] Bigelow Lab Ocean Sci, West Boothbay Harbor, ME USA. [Feldman, Gene] NASA, Goddard Space Flight Ctr, SeaWiFS, Greenbelt, MD 20771 USA. [Swift, Calvin] Univ Massachusetts, Amherst, MA 01003 USA. RP Lagerloef, G (reprint author), NASA, Aquarius Miss Earth & Space Res, Seattle, WA USA. EM lager@esr.org RI Ruf, Christopher/I-9463-2012 NR 23 TC 197 Z9 205 U1 0 U2 12 PU OCEANOGRAPHY SOC PI ROCKVILLE PA P.O. BOX 1931, ROCKVILLE, MD USA SN 1042-8275 J9 OCEANOGRAPHY JI Oceanography PD MAR PY 2008 VL 21 IS 1 BP 68 EP 81 PG 14 WC Oceanography SC Oceanography GA 382XJ UT WOS:000261638400012 ER PT J AU Boyer, T Carton, J Chao, Y Gordon, A Johnson, G Lagerloef, G Large, B Riser, S Schmitt, R AF Boyer, Tim Carton, Jim Chao, Yi Gordon, Arnold Johnson, Greg Lagerloef, Gary Large, Bill Riser, Steve Schmitt, Ray CA CLIVAR Salinity Working Grp TI What's Next for Salinity? SO OCEANOGRAPHY LA English DT Article C1 [Carton, Jim] Univ Maryland, College Pk, MD 20742 USA. [Chao, Yi] NASA, Jet Prop Lab, Washington, DC USA. [Gordon, Arnold] Columbia Univ, Lamont Doherty Earth Observ, New York, NY 10027 USA. [Riser, Steve] Univ Washington, Seattle, WA 98195 USA. [Schmitt, Ray] Woods Hole Oceanog Inst, Woods Hole, MA 02543 USA. EM rschmitt@whoi.edu RI carton, james/C-4807-2009 OI carton, james/0000-0003-0598-5198 FU NASA FX The Salinity Working Group recognizes Cathy Stephens and David Legler of the US CLIVAR Office as well as Eric Lindstrom of NASA for their Support activities. NR 0 TC 0 Z9 1 U1 0 U2 2 PU OCEANOGRAPHY SOC PI ROCKVILLE PA P.O. BOX 1931, ROCKVILLE, MD USA SN 1042-8275 J9 OCEANOGRAPHY JI Oceanography PD MAR PY 2008 VL 21 IS 1 BP 82 EP 85 PG 4 WC Oceanography SC Oceanography GA 382XJ UT WOS:000261638400013 ER PT J AU Hofmann, E Druon, JN Fennel, K Friedrichs, M Haidvogel, D Lee, C Mannino, A McClain, C Najjar, R O'Reilly, J Pollard, D Previdi, M Seitzinger, S Siewert, J Signorini, S Wilkin, J AF Hofmann, Eileen Druon, Jean-Noel Fennel, Katja Friedrichs, Marjorie Haidvogel, Dale Lee, Cindy Mannino, Antonio McClain, Charles Najjar, Raymond O'Reilly, John Pollard, David Previdi, Michael Seitzinger, Sybil Siewert, John Signorini, Sergio Wilkin, John CA USECoS Team TI EASTERN US CONTINENTAL SHELF CARBON BUDGET Integrating Models, Data Assimilation, and Analysis SO OCEANOGRAPHY LA English DT Article ID DISSOLVED ORGANIC-CARBON; CZCS-CHLOROPHYLL IMAGERY; WARM-CORE RING; ATLANTIC BIGHT; OCEAN COLOR; ECOSYSTEM MODEL; DEEP-OCEAN; MATTER; PHYTOPLANKTON; PARTICULATE C1 [Hofmann, Eileen] Old Dominion Univ, Dept Ocean Earth & Atmospher Sci, Norfolk, VA USA. [Druon, Jean-Noel; Mannino, Antonio; McClain, Charles] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Fennel, Katja] Dalhousie Univ, Dept Oceanog, Halifax, NS, Canada. [Friedrichs, Marjorie] Virginia Inst Marine Sci, Gloucester Point, VA 23062 USA. [Haidvogel, Dale; Previdi, Michael; Seitzinger, Sybil; Wilkin, John] Rutgers State Univ, Inst Marine & Coastal Sci, New Brunswick, NJ 08903 USA. [Lee, Cindy] SUNY Stony Brook, Marine Sci Res Ctr, Stony Brook, NY 11794 USA. [Najjar, Raymond; Siewert, John] Penn State Univ, Dept Meteorol, University Pk, PA 16802 USA. [O'Reilly, John] NOAA, Natl Marine Fisheries Serv, Narragansett Lab, Narragansett, RI 02882 USA. [Pollard, David] Penn State Univ, Earth & Environm Syst Inst, State Coll, PA USA. [Signorini, Sergio] Sci Applicat Int Corp, Beltsville, MD USA. RP Hofmann, E (reprint author), Old Dominion Univ, Dept Ocean Earth & Atmospher Sci, Norfolk, VA USA. EM hofmann@ccpo.odu.edu RI Fennel, Katja/A-7470-2009; Lee, Cindy/B-1456-2009; Wilkin, John/E-5343-2011; Mannino, Antonio/I-3633-2014; OI Fennel, Katja/0000-0003-3170-2331; Lee, Cindy/0000-0002-7608-6213; Wilkin, John/0000-0002-5444-9466; Friedrichs, Marjorie/0000-0003-2828-7595 FU National Aeronautics and Space Administration Interdisciplinary Science Program FX The USECoS project is Supported by the National Aeronautics and Space Administration Interdisciplinary Science Program. NR 65 TC 19 Z9 19 U1 0 U2 12 PU OCEANOGRAPHY SOC PI ROCKVILLE PA P.O. BOX 1931, ROCKVILLE, MD USA SN 1042-8275 J9 OCEANOGRAPHY JI Oceanography PD MAR PY 2008 VL 21 IS 1 BP 86 EP 104 PG 19 WC Oceanography SC Oceanography GA 382XJ UT WOS:000261638400014 ER PT J AU Trigwell, S Biris, AS Sims, RA Mazumder, MK AF Trigwell, Steve Biris, A. S. Sims, Robert A. Mazumder, Malay K. TI Effects of powder velocity and contact materials on tribocharging of polymer powders for powder coating applications SO PARTICULATE SCIENCE AND TECHNOLOGY LA English DT Article DE back corona; charge-to-mass; Faraday penetration; powders; tribocharging ID ELECTRIFICATION AB Electrostatic powder deposition using corona charging is widely used in a plethora of industrial applications. Disadvantages of this technique are back corona onset and the Faraday penetration limitation. Another method to charge powders is to use tribochargers. Tribocharging depends upon the work function difference between the contacting materials and generates bipolarly charged particles. In this study, acrylic and epoxy powders were fluidized and charged by passing through stainless steel, copper, aluminum, and polycarbonate static mixers, respectively. The particle velocity and powder flow rate were varied to determine their effect on the net charge-to-mass ratio (Q/M) acquired by the powders. The Q/M increased rapidly with velocities between 1.5 to 2.5 m/s and stabilized for higher velocities but decreased with increasing powder flow rate at a constant velocity. The net positive or negative charge on each powder was determined to be dependant on the charger material. The use of an aluminum charger (net negative charge) in combination with a PTFE finger nozzle (net positive charge) resulted in a net powder Q/M of -0.05 mu C/g. The generation of an ion-free powder cloud with high bipolar charge but overall charge density of almost zero is anticipated to provide a better coverage of recessed areas. C1 [Trigwell, Steve] NASA, Kennedy Space Ctr, Electrostat & Surface Phys Lab, ASRC Aerosp 24, Kennedy Space Ctr, FL 32899 USA. [Biris, A. S.; Sims, Robert A.; Mazumder, Malay K.] Univ Arkansas, Dept Appl Sci, Little Rock, AR 72204 USA. RP Trigwell, S (reprint author), NASA, Kennedy Space Ctr, Electrostat & Surface Phys Lab, ASRC Aerosp 24, Mail Stop ASRC-20, Kennedy Space Ctr, FL 32899 USA. EM steven.trigwell-l@nasa.gov RI Biris, Alexandru/A-8507-2010 NR 16 TC 4 Z9 4 U1 1 U2 3 PU TAYLOR & FRANCIS INC PI PHILADELPHIA PA 325 CHESTNUT ST, SUITE 800, PHILADELPHIA, PA 19106 USA SN 0272-6351 J9 PARTICUL SCI TECHNOL JI Part. Sci. Technol. PD MAR-APR PY 2008 VL 26 IS 2 BP 145 EP 157 DI 10.1080/02726350801890946 PG 13 WC Engineering, Chemical SC Engineering GA 286HL UT WOS:000254836900005 ER PT J AU Huang, SL Rich, PM Crabtree, RL Potter, CS Fu, PD AF Huang, Shengli Rich, Paul M. Crabtree, Robert L. Potter, Christopher S. Fu, Pinde TI Modeling monthly near-surface air temperature from solar radiation and lapse rate: Application over complex terrain in Yellowstone National Park SO PHYSICAL GEOGRAPHY LA English DT Article DE montane ecosystem; solar radiation; surface temperature; Yellowstone National Park ID INTERPOLATION; PRECIPITATION; SIMULATION; VEGETATION; ECOSYSTEM; REGIONS; SITES AB Spatially distributed surface temperature over complex topography is important to many ecological processes, but it varies spatially and temporally in complex ways and is difficult to measure at landscape scales at tens of meters resolution. Our goal is to develop a methodology that accurately predicts Surface temperature in mountain ecosystems. First, we modeled monthly incoming solar radiation (insolation) based on topography and observed variation in atmospheric conditions, and accounting for site latitude, elevation, and Surface orientation (slope and aspect), daily and seasonal shifts in sun angle, and effects of shadows cast by surrounding topography. Then we investigated the ability to predict monthly average temperature from lapse rates together with energy input from insolation. Monthly lapse rates are not constant and have a seasonal variation. Monthly temperature is not highly correlated with the corresponding monthly insolation; however, it is highly correlated with a one-month-lag insolation, enabling calculation of a lag-corrected linear regression. We used this regression to calculate 30 m resolution surface temperature maps for mountain areas at Yellowstone National Park. The comparison between our modeled temperature and observed temperature shows the mean average errors range from 0.90 degrees C to 1.49 degrees C. Our approach, with consideration of influences of topography and variable atmospheric conditions on energy from insolation, and with appropriate time lags, greatly improves the ability to calculate spatially distributed temperature regimes in complex terrain. C1 [Huang, Shengli; Potter, Christopher S.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Huang, Shengli; Crabtree, Robert L.] Yellowstone Ecol Res Ctr, Bozeman, MT 59718 USA. [Rich, Paul M.] Creekside Ctr Earth Observat, Menlo Pk, CA 94025 USA. [Fu, Pinde] ESRI Inc, Redlands, CA 92373 USA. RP Huang, SL (reprint author), NASA, Ames Res Ctr, Mail Stop 242-4, Moffett Field, CA 94035 USA. FU NASA [NNS06AA23G] FX We thank NASA for providing the financial support (contract No. NNS06AA23G). This research was also 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. We also thank Mrs. Met Peng for collecting and pre-processing weather data and Mrs. Diane Ehernberger for carefully improving the English. NR 38 TC 18 Z9 20 U1 2 U2 13 PU BELLWETHER PUBL LTD PI COLUMBIA PA 8640 GUILFORD RD, STE 200, COLUMBIA, MD 21046 USA SN 0272-3646 J9 PHYS GEOGR JI Phys. Geogr. PD MAR-APR PY 2008 VL 29 IS 2 BP 158 EP 178 DI 10.2747/0272-3646.29.2.158 PG 21 WC Environmental Sciences; Geography, Physical; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Environmental Sciences & Ecology; Physical Geography; Geology; Meteorology & Atmospheric Sciences GA 352PE UT WOS:000259508500004 ER PT J AU Abbott, B Abbott, R Adhikari, R Agresti, J Ajith, P Allen, B Amin, R Anderson, SB Anderson, WG Arain, M Araya, M Armandula, H Ashley, M Aston, S Aufmuth, P Aulbert, C Babak, S Ballmer, S Bantilan, H Barish, BC Barker, C Barker, D Barr, B Barriga, P Barton, MA Bayer, K Belczynski, K Berukoff, SJ Betzwieser, J Beyersdorf, PT Bhawal, B Bilenko, IA Billingsley, G Biswas, R Black, E Blackburn, K Blackburn, L Blair, D Bland, B Bogenstahl, J Bogue, L Bork, R Boschi, V Bose, S Brady, PR Braginsky, VB Brau, JE Brinkmann, M Brooks, A Brown, DA Bullington, A Bunkowski, A Buonanno, A Burmeister, O Busby, D Butler, WE Byer, RL Cadonati, L Cagnoli, G Camp, JB Cannizzo, J Cannon, K Cantley, CA Cao, J Cardenas, L Carter, K Casey, MM Castaldi, G Cepeda, C Chalkley, E Charlton, P Chatterji, S Chelkowski, S Chen, Y Chiadini, F Chin, D Chin, E Chow, J Christensen, N Clark, J Cochrane, P Cokelaer, T Colacino, CN Coldwell, R Coles, M Conte, R Cook, D Corbitt, T Coward, D Coyne, D Creighton, JDE Creighton, TD Croce, RP Crooks, DRM Cruise, AM Csatorday, P Cumming, A Dalrymple, J D'Ambrosio, E Danzmann, K Davies, G Daw, E Debra, D Degallaix, J Degree, M Delker, T Demma, T Dergachev, V Desai, S DeSalvo, R Dhurandhar, S Daiz, M Dickson, J Di Credico, A Diederichs, G Dietz, A Ding, H Doomes, EE Drever, RWP Dumas, JC Dupuis, RJ Dwyer, JG Ehrens, P Espinoza, E Etzel, T Evans, M Evans, T Fairhurst, S Fan, Y Fazi, D Fejer, MM Finn, LS Fiumara, V Fotopoulos, N Franzen, A Franzen, KY Freise, A Frey, R Fricke, T Fritschel, P Frolov, VV Fyffe, M Galdi, V Ganezer, KS Garofoli, J Gholami, I Giaime, JA Giampanis, S Giardina, KD Goda, K Goetz, E Goggin, L Gonzalez, G Gossler, S Grant, A Gras, S Gray, C Gray, M Greenhalgh, J Gretarsson, AM Grosso, R Grote, H Grunewald, S Guenther, M Gustafson, R Hage, B Hammer, D Hanna, C Hanson, J Harms, J Harry, G Harstad, E Hayler, T Heefner, J Heinzel, G Heng, IS Heptonstall, A Heurs, M Hewitson, M Hirose, E Hoak, D Hosken, D Hough, J Howell, E Hoyland, D Huttner, SH Ingram, D Innerhofer, E Ito, M Itoh, Y Ivanov, A Jackrel, D Jennrich, O Johnson, B Johnson, WW Johnston, WR Jones, DI Jones, G Jones, R Ju, L Kalmus, P Kalogera, V Kasprzyk, D Katsavounidis, E Kawabe, K Kawamura, S Kawazoe, F Kells, W Keppel, DG Khalili, FY Killow, CJ Kim, C King, P Kissel, JS Klimenko, S Kokeyama, K Kondrashov, V Kopparapu, RK Kozak, D Krishnan, B Kwee, P Lam, PK Landry, M Lantz, B Lazzarini, A Lee, B Lei, M Leiner, J Leonhardt, V Leonor, I Libbrecht, K Libson, A Lindquist, P Lockerbie, NA Logan, J Longo, M Lormand, M Lubinski, M Luck, H Machenschalk, B MacInnis, M Mageswaran, M Mailand, K Malec, M Mandic, V Marano, S Marka, S Markowitz, J Maros, E Martin, I Marx, JN Mason, K Matone, L Matta, V Mavalvala, N McCarthy, R McClelland, DE McGuire, SC McHugh, M McKenzie, K McNabb, JWC McWilliams, S Meier, T Melissinos, A Mendell, G Mercer, RA Meshkov, S Messaritaki, E Messenger, CJ Meyers, D Mikhailov, E Mitra, S Mitrofanov, VP Mitselmakher, G Mittleman, R Miyakawa, O Mohanty, S Moreno, G Mossavi, K MowLowry, C Moylan, A Mudge, D Mueller, G Mukherjee, S Muller-Ebhardt, H Munch, J Murray, P Myers, E Myers, J Nagano, S Nash, T Newton, G Nishizawa, A Nocera, F Numata, K Nutzman, P O'Reilly, B O'Shaughnessy, R Ottaway, DJ Overmier, H Owen, BJ Pan, Y Papa, MA Parameshwaraiah, V Parameswariah, C Patel, P Pedraza, M Penn, S Pierro, V Pinto, IM Pitkin, M Pletsch, H Plissi, MV Postiglione, F Prix, R Quetschke, V Raab, F Rabeling, D Radkins, H Rahkola, R Rainer, N Rakhmanov, M Ramsunder, M Rawlins, K Ray-Majumder, S Re, V Regimbau, T Rehbein, H Reid, S Reitze, DH Ribichini, L Richman, S Riesen, R Riles, K Rivera, B Robertson, NA Robinson, C Robinson, EL Roddy, S Rodriguez, A Rogan, AM Rollins, J Romano, JD Romie, J Rong, H Route, R Rowan, S Rudieger, A Ruet, L Russell, P Ryan, K Sakata, S Samidi, M de la Jordana, LS Sandberg, V Sanders, GH Sannibale, V Saraf, S Sarin, P Sathyaprakash, BS Sato, S Saulson, PR Savage, R Savov, P Sazonov, A Schediwy, S 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 Sidles, JA Siemens, X Sigg, D Sinha, S Sintes, AM Slagmolen, BJJ Slutsky, J Smith, JR Smith, MR Somiya, K Strain, KA Strand, NE Strom, DM Stuver, A Summerscales, TZ Sun, KX Sung, M Sutton, PJ Sylvestre, J Takahashi, H Takamori, A Tanner, DB Tarallo, M Taylor, R Taylor, R Thacker, J Thorne, KA Thorne, KS Thuring, A Tinto, M Tokmakov, KV Torres, C Torrie, C Traylor, G Trias, M Tyler, W Ugolini, D Ungarelli, C Urbanek, K Vahlbruch, H Vallisneri, M Van Den Broeck, C van Putten, M Varvella, M Vass, S Vecchio, A Veitch, J Veitch, P Villar, A Vorvick, C Vyachanin, SP Waldman, SJ Wallace, L Ward, H Ward, R Watts, K Webber, D Weidner, A Weinert, M Weinstein, A Weiss, R Wen, L Wen, S Wette, K Whelan, JT Whitbeck, DM Whitcomb, SE Whiting, BF Wiley, S Wilkinson, C Willems, PA Williams, L Willke, B Wilmut, I Winkler, W Wipf, CC Wise, S Wiseman, AG Woan, G Woods, D Wooley, R Worden, J Wu, W Yakushin, I Yamamoto, H Yan, Z Yoshida, S Yunes, N Zaleski, KD Zanolin, M Zhang, J Zhang, L Zhao, C Zotov, N Zucker, M Muhlen, HZ Zweizig, J Hild, S AF Abbott, B. Abbott, R. Adhikari, R. Agresti, J. Ajith, P. Allen, B. Amin, R. Anderson, S. B. Anderson, W. G. Arain, M. Araya, M. Armandula, H. Ashley, M. 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. Bayer, K. Belczynski, K. Berukoff, S. J. Betzwieser, J. Beyersdorf, P. T. Bhawal, B. Bilenko, I. A. Billingsley, G. Biswas, R. Black, E. Blackburn, K. Blackburn, L. Blair, D. Bland, B. Bogenstahl, J. Bogue, L. Bork, R. Boschi, V. Bose, S. Brady, P. R. Braginsky, V. B. Brau, J. E. Brinkmann, M. Brooks, A. Brown, D. A. Bullington, A. Bunkowski, A. Buonanno, A. Burmeister, O. Busby, D. Butler, W. E. Byer, R. L. Cadonati, L. Cagnoli, G. Camp, J. B. Cannizzo, J. Cannon, K. Cantley, C. A. Cao, J. Cardenas, L. Carter, K. Casey, M. M. Castaldi, G. Cepeda, C. Chalkley, E. Charlton, P. Chatterji, S. Chelkowski, S. Chen, Y. Chiadini, F. Chin, D. Chin, E. Chow, J. Christensen, N. Clark, J. Cochrane, P. Cokelaer, T. Colacino, C. N. Coldwell, R. Coles, M. Conte, R. Cook, D. Corbitt, T. Coward, D. Coyne, D. Creighton, J. D. E. Creighton, T. D. Croce, R. P. Crooks, D. R. M. Cruise, A. M. Csatorday, P. Cumming, A. Dalrymple, J. D'Ambrosio, E. Danzmann, K. Davies, G. Daw, E. DeBra, D. Degallaix, J. Degree, M. Delker, T. Demma, T. Dergachev, V. Desai, S. DeSalvo, R. Dhurandhar, S. Daiz, M. Dickson, J. Di Credico, A. Diederichs, G. Dietz, A. Ding, H. Doomes, E. E. Drever, R. W. P. Dumas, J. -C. Dupuis, R. J. Dwyer, J. G. Ehrens, P. Espinoza, E. Etzel, T. Evans, M. Evans, T. Fairhurst, S. Fan, Y. Fazi, D. Fejer, M. M. Finn, L. S. Fiumara, V. Fotopoulos, N. Franzen, A. Franzen, K. Y. Freise, A. Frey, R. Fricke, T. Fritschel, P. Frolov, V. V. Fyffe, M. Galdi, V. Ganezer, K. S. Garofoli, J. Gholami, I. Giaime, J. A. Giampanis, S. Giardina, K. D. Goda, K. Goetz, E. Goggin, L. Gonzalez, G. Gossler, S. Grant, A. Gras, S. Gray, C. Gray, M. Greenhalgh, J. Gretarsson, A. M. Grosso, R. Grote, H. Grunewald, S. Guenther, M. Gustafson, R. Hage, B. Hammer, D. Hanna, C. Hanson, J. Harms, J. Harry, G. Harstad, E. Hayler, T. Heefner, J. Heinzel, G. Heng, I. S. Heptonstall, A. Heurs, M. Hewitson, M. Hirose, E. Hoak, D. Hosken, D. Hough, J. Howell, E. Hoyland, D. Huttner, S. H. Ingram, D. Innerhofer, E. Ito, M. Itoh, Y. Ivanov, A. Jackrel, D. Jennrich, O. Johnson, B. Johnson, W. W. Johnston, W. R. Jones, D. I. Jones, G. Jones, R. Ju, L. Kalmus, P. Kalogera, V. Kasprzyk, D. Katsavounidis, E. Kawabe, K. Kawamura, S. Kawazoe, F. Kells, W. Keppel, D. G. Khalili, F. Ya. Killow, C. J. Kim, C. King, P. Kissel, J. S. Klimenko, S. Kokeyama, K. Kondrashov, V. Kopparapu, R. K. Kozak, D. Krishnan, B. Kwee, P. Lam, P. K. Landry, M. Lantz, B. Lazzarini, A. Lee, B. Lei, M. Leiner, J. Leonhardt, V. Leonor, I. Libbrecht, K. Libson, A. Lindquist, P. Lockerbie, N. A. Logan, J. Longo, M. Lormand, M. Lubinski, M. Lueck, H. Machenschalk, B. MacInnis, M. Mageswaran, M. Mailand, K. Malec, M. Mandic, V. Marano, S. Marka, S. Markowitz, J. Maros, E. Martin, I. Marx, J. N. Mason, K. Matone, L. Matta, V. Mavalvala, N. McCarthy, R. McClelland, D. E. McGuire, S. C. McHugh, M. McKenzie, K. McNabb, J. W. C. McWilliams, S. Meier, T. Melissinos, A. Mendell, G. Mercer, R. A. Meshkov, S. Messaritaki, E. Messenger, C. J. Meyers, D. Mikhailov, E. Mitra, S. Mitrofanov, V. P. Mitselmakher, G. Mittleman, R. Miyakawa, O. Mohanty, S. Moreno, G. Mossavi, K. MowLowry, C. Moylan, A. Mudge, D. Mueller, G. Mukherjee, S. Mueller-Ebhardt, H. Munch, J. Murray, P. Myers, E. Myers, J. Nagano, S. Nash, T. Newton, G. Nishizawa, A. Nocera, F. Numata, K. Nutzman, P. O'Reilly, B. O'Shaughnessy, R. Ottaway, D. J. Overmier, H. Owen, B. J. Pan, Y. Papa, M. A. Parameshwaraiah, V. Parameswariah, C. Patel, P. Pedraza, M. Penn, S. Pierro, V. Pinto, I. M. Pitkin, M. Pletsch, H. Plissi, M. V. Postiglione, F. Prix, R. Quetschke, V. Raab, F. Rabeling, D. Radkins, H. Rahkola, R. Rainer, N. Rakhmanov, M. Ramsunder, M. Rawlins, K. Ray-Majumder, S. Re, V. Regimbau, T. Rehbein, H. Reid, S. Reitze, D. H. Ribichini, L. Richman, S. 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. Rong, H. Route, R. Rowan, S. Ruedieger, A. Ruet, L. Russell, P. Ryan, K. Sakata, S. Samidi, M. de la Jordana, L. Sancho Sandberg, V. Sanders, G. H. Sannibale, V. Saraf, S. Sarin, P. Sathyaprakash, B. S. Sato, S. Saulson, P. R. Savage, R. Savov, P. Sazonov, A. Schediwy, S. 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. Sidles, J. A. Siemens, X. Sigg, D. Sinha, S. Sintes, A. M. Slagmolen, B. J. J. Slutsky, J. Smith, J. R. Smith, M. R. Somiya, K. Strain, K. A. Strand, N. E. Strom, D. M. Stuver, A. Summerscales, T. Z. Sun, K. -X. Sung, M. Sutton, P. J. Sylvestre, J. Takahashi, H. Takamori, A. Tanner, D. B. Tarallo, M. 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. Ungarelli, C. Urbanek, K. Vahlbruch, H. Vallisneri, M. Van Den Broeck, C. van Putten, M. Varvella, M. Vass, S. Vecchio, A. Veitch, J. Veitch, P. Villar, A. Vorvick, C. Vyachanin, S. P. Waldman, S. J. Wallace, L. Ward, H. Ward, R. Watts, K. Webber, D. Weidner, A. Weinert, M. Weinstein, A. Weiss, R. Wen, L. Wen, S. Wette, K. Whelan, J. T. Whitbeck, D. M. Whitcomb, S. E. Whiting, B. F. Wiley, S. Wilkinson, C. Willems, P. A. Williams, L. Willke, B. Wilmut, I. Winkler, W. Wipf, C. C. Wise, S. Wiseman, A. G. Woan, G. Woods, D. Wooley, R. Worden, J. Wu, W. Yakushin, I. Yamamoto, H. Yan, Z. Yoshida, S. Yunes, N. Zaleski, K. D. Zanolin, M. Zhang, J. Zhang, L. Zhao, C. Zotov, N. Zucker, M. Muehlen, H. zur Zweizig, J. Hild, S. TI Search for gravitational waves associated with 39 gamma-ray bursts using data from the second, third, and fourth LIGO runs SO PHYSICAL REVIEW D LA English DT Article ID 25 APRIL 1998; SHORT-DURATION GRBS; SIGNAL-TO-NOISE; CORE-COLLAPSE; REDSHIFT DISTRIBUTIONS; UNUSUAL SUPERNOVA; FORMATION RATES; STAR-FORMATION; NEUTRON-STARS; ERROR BOX AB We present the results of a search for short-duration gravitational-wave bursts associated with 39 gamma-ray bursts (GRBs) detected by gamma-ray satellite experiments during LIGO's S2, S3, and S4 science runs. The search involves calculating the crosscorrelation between two interferometer data streams surrounding the GRB trigger time. We search for associated gravitational radiation from single GRBs, and also apply statistical tests to search for a gravitational-wave signature associated with the whole sample. For the sample examined, we find no evidence for the association of gravitational radiation with GRBs, either on a single-GRB basis or on a statistical basis. Simulating gravitational-wave bursts with sine-Gaussian waveforms, we set upper limits on the root-sum-square of the gravitational-wave strain amplitude of such waveforms at the times of the GRB triggers. We also demonstrate how a sample of several GRBs can be used collectively to set constraints on population models. The small number of GRBs and the significant change in sensitivity of the detectors over the three runs, however, limits the usefulness of a population study for the S2, S3, and S4 runs. Finally, we discuss prospects for the search sensitivity for the ongoing S5 run, and beyond for the next generation of detectors. C1 [Abbott, B.; Abbott, R.; Adhikari, R.; Agresti, J.; Anderson, S. B.; Araya, M.; Armandula, H.; Ballmer, S.; Barish, B. C.; Bhawal, B.; Billingsley, G.; Black, E.; Blackburn, K.; Bork, R.; Boschi, V.; Brown, D. A.; Busby, D.; Cardenas, L.; Cepeda, C.; Chatterji, S.; Coyne, D.; D'Ambrosio, E.; Drever, R. W. P.; Dupuis, R. J.; Goggin, L.; Heefner, J.; Ivanov, A.; Kells, W.; Keppel, D. G.; King, P.; Kondrashov, V.; Kozak, D.; Lazzarini, A.; Lei, M.; Libbrecht, K.; Lindquist, P.; Logan, J.; Mageswaran, M.; Mailand, K.; Mandic, V.; Maros, E.; Marx, J. N.; Meshkov, S.; Messaritaki, E.; Meyers, D.; Miyakawa, O.; Nash, T.; Nocera, F.; Patel, P.; Pedraza, M.; Robertson, N. A.; Russell, P.; Samidi, M.; Sanders, G. H.; Sannibale, V.; Sears, B.; Siemens, X.; Smith, M. R.; Sutton, P. J.; Sylvestre, J.; Takamori, A.; Tarallo, M.; Taylor, R.; Tyler, W.; Waldman, S. J.; Wallace, L.; Ward, R.; Webber, D.; Weinstein, A.; Yamamoto, H.; Zhang, L.; Zweizig, J.] CALTECH, LIGO, Pasadena, CA 91125 USA. [Aulbert, C.; Babak, S.; Berukoff, S. J.; Chen, Y.; Gholami, I.; Krishnan, B.; Machenschalk, B.; Papa, M. A.; Prix, R.; Schutz, B. F.; Sintes, A. M.; Somiya, K.; Takahashi, H.; Wen, L.; Whelan, J. T.] Max Planck Inst Gravitat Phys, Albert Einstein Inst, D-30167 Hannover, Germany. [Ajith, P.; Allen, B.; Brinkmann, M.; Bunkowski, A.; Burmeister, O.; Chelkowski, S.; Cochrane, P.; Danzmann, K.; Harms, J.; Heinzel, G.; Heurs, M.; Hewitson, M.; Lueck, H.; Mossavi, K.; Mueller-Ebhardt, H.; Nagano, S.; Pletsch, H.; Rainer, N.; Rehbein, H.; Ribichini, L.; Ruedieger, A.; Schilling, R.; Schnabel, R.; Seifert, F.; Smith, J. R.; Somiya, K.; Weidner, A.; 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. [Ashley, M.; Chow, J.; Gossler, S.; Gray, M.; Lam, P. K.; McClelland, D. E.; McKenzie, K.; MowLowry, C.; Moylan, A.; Rabeling, D.; Scott, S. M.; Searle, A. C.; Slagmolen, B. J. J.; Wette, K.] Australian Natl Univ, Canberra, ACT 0200, Australia. [Ganezer, K. S.; Wiley, S.] Calif State Univ Dominguez Hills, Carson, CA 90747 USA. [Brown, D. A.; Savov, P.; Siemens, X.; Thorne, K. S.; Vallisneri, M.] CALTECH, CaRT, Pasadena, CA 91125 USA. [Cokelaer, T.; Davies, G.; Jones, G.; Regimbau, T.; Romano, J. D.; Sathyaprakash, B. S.; Sengupta, A. S.; Van Den Broeck, C.] Cardiff Univ, Cardiff CF24 3AA, Wales. [Bantilan, H.; Christensen, N.; Libson, A.] Carleton Coll, Northfield, MN 55057 USA. [Charlton, P.] Charles Sturt Univ, Wagga Wagga, NSW 2678, Australia. [Dwyer, J. G.; Kalmus, P.; Marka, S.; Matone, L.; Rollins, J.] Columbia Univ, New York, NY 10027 USA. [Gretarsson, A. M.] Embry Riddle Aeronaut Univ, Prescott, AZ 86301 USA. [Penn, S.] Hobart & William Smith Coll, Geneva, NY 14456 USA. [Mitra, S.; Varvella, M.; Vass, S.; Villar, A.] Inter Univ Ctr Astron & Astrophys, Pune 411007, Maharashtra, India. 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[Bayer, K.; Betzwieser, J.; Blackburn, L.; Cadonati, L.; Cao, J.; Corbitt, T.; Csatorday, P.; Fritschel, P.; Goda, K.; Harstad, E.; Innerhofer, E.; Katsavounidis, E.; MacInnis, M.; Markowitz, J.; Mason, K.; Mavalvala, N.; Mikhailov, E.; Mittleman, R.; Ottaway, D. J.; Rawlins, K.; Richman, S.; Ruet, L.; Sarin, P.; Shoemaker, D. H.; van Putten, M.; Weiss, R.; Wipf, C. C.; Zanolin, M.; Zucker, M.] MIT, LIGO, Cambridge, MA 02139 USA. [Amin, R.; Giaime, J. A.; Gonzalez, G.; Johnson, W. W.; Kissel, J. S.; Kopparapu, R. K.; 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. [McHugh, M.] Loyola Univ, New Orleans, LA 70118 USA. Max Planck Inst Quantum Opt, D-85748 Garching, Germany. [Bilenko, I. A.; Braginsky, V. B.; Khalili, F. Ya.; Mitrofanov, V. P.] Moscow MV Lomonosov State Univ, Moscow 119992, Russia. [Camp, J. B.; Cannizzo, J.; McWilliams, S.; Numata, K.; Vyachanin, S. P.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Kawamura, S.; Kawazoe, F.; Kokeyama, K.; Leonhardt, V.; Nishizawa, A.; Sakata, S.; Sato, S.] Natl Astron Observ, Tokyo 1818588, Japan. [Belczynski, K.; Kalogera, V.; Kim, C.; Nutzman, P.; O'Shaughnessy, R.] Northwestern Univ, Evanston, IL 60208 USA. [Saraf, S.] Rochester Inst Technol, Rochester, NY 14623 USA. [Greenhalgh, J.; Hayler, T.; Wilmut, I.] Rutherford Appleton Lab, Didcot OX11 0QX, Oxon, England. [Beyersdorf, P. T.] San Jose State Univ, San Jose, CA 95192 USA. [Yoshida, S.] SE Louisiana Univ, Hammond, LA 70402 USA. [Doomes, E. E.; McGuire, S. C.] So Unit & A&M Univ, Baton Rouge, LA 70813 USA. [Bullington, A.; Byer, R. L.; DeBra, D.; Degree, M.; Jackrel, D.; Lantz, B.; Rowan, S.; Sinha, S.; Sun, K. -X.; Urbanek, K.] Stanford Univ, Stanford, CA 94305 USA. [Dalrymple, J.; Hirose, E.; Saulson, P. R.] Syracuse Univ, Syracuse, NY 13244 USA. [Desai, S.; Finn, L. S.; McNabb, J. W. C.; Owen, B. 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[Arain, M.; Coldwell, R.; Delker, T.; Franzen, K. Y.; Klimenko, S.; Mercer, R. A.; Mitselmakher, G.; Mueller, G.; Quetschke, V.; Reitze, D. H.; Rong, H.; Sazonov, A.; Williams, L.; Wise, S.; Wu, W.] Univ Florida, Gainesville, FL 32611 USA. [Barr, B.; Barton, M. A.; Cagnoli, G.; Cantley, C. A.; Casey, M. M.; Chalkley, E.; Clark, J.; Crooks, D. R. M.; Cumming, A.; Grant, A.; Heinzel, G.; Heng, I. S.; Heptonstall, A.; Huttner, S. H.; Jennrich, O.; Jones, R.; Killow, C. J.; Martin, I.; Messenger, C. J.; Murray, P.; Newton, G.; Pitkin, M.; Plissi, M. V.; Reid, S.; Robertson, N. A.; Strain, K. A.; Taylor, R.; Tokmakov, K. V.; Torrie, C.; Veitch, J.; Ward, H.; Whiting, B. F.; Woan, G.] Univ Glasgow, Glasgow G12 8QQ, Lanark, Scotland. [Bogenstahl, J.; Buonanno, A.; Pan, Y.; Shawhan, P.] Univ Maryland, College Pk, MD 20742 USA. [Chin, D.; Dergachev, V.; Goetz, E.; Riles, K.; Zhang, J.] Univ Michigan, Ann Arbor, MI 48109 USA. [Brau, J. E.; Frey, R.; Ito, M.; Leonor, I.; Rahkola, R.; Schofield, R.; Strom, D. M.] Univ Oregon, Eugene, OR 97403 USA. [Butler, W. E.; Fricke, T.; Giampanis, S.; Melissinos, A.] Univ Rochester, Rochester, NY 14627 USA. [Chiadini, F.; Conte, R.; Fiumara, V.; Longo, M.; Marano, S.; Matta, V.; Postiglione, F.] Univ Salerno, I-84084 Salerno, Italy. [Castaldi, G.; Croce, R. P.; Demma, T.; Galdi, V.; Pierro, V.; Pinto, I. M.] Univ Sannio, I-82100 Benevento, Italy. [Daw, E.] Univ Sheffield, Sheffield S3 7RH, S Yorkshire, England. [Jones, D. I.] Univ Southampton, Southampton SO17 1BJ, Hants, England. [Lockerbie, N. A.] Univ Strathclyde, Glasgow G1 1XQ, Lanark, Scotland. [Sidles, J. A.] Univ Washington, Seattle, WA 98195 USA. [Barriga, P.; Blair, D.; Chin, E.; Coward, D.; Degallaix, J.; Dumas, J. -C.; Gras, S.; Howell, E.; Ju, L.; Lee, B.; Schediwy, S.; Yan, Z.; Zhao, C.] Univ Western Australia, Crawley, NSW 6009, Australia. [Allen, B.; Anderson, W. G.; Biswas, R.; Brady, P. R.; Cannon, K.; Creighton, J. D. E.; Creighton, T. D.; Fotopoulos, N.; Itoh, Y.; Papa, M. A.; Ray-Majumder, S.; Wiseman, A. G.; Woods, D.] Univ Wisconsin, Milwaukee, WI 53201 USA. Vassar Coll, Poughkeepsie, NY 12604 USA. [Bose, S.; Leiner, J.; Rogan, A. M.] Washington State Univ, Pullman, WA 99164 USA. RP Abbott, B (reprint author), CALTECH, LIGO, Pasadena, CA 91125 USA. RI Harms, Jan/J-4359-2012; Chow, Jong/A-3183-2008; Frey, Raymond/E-2830-2016; Howell, Eric/H-5072-2014; Ward, Robert/I-8032-2014; Lueck, Harald/F-7100-2011; Lam, Ping Koy/A-5276-2008; Galdi, Vincenzo/B-1670-2008; Sylvestre, Julien/A-8610-2009; McClelland, David/E-6765-2010; Martin, Iain/A-2445-2010; Hild, Stefan/A-3864-2010; Schutz, Bernard/B-1504-2010; Casey, Morag/C-9703-2010; Rowan, Sheila/E-3032-2010; Strain, Kenneth/D-5236-2011; Raab, Frederick/E-2222-2011; Biswas, Rahul/H-7474-2016; Re, Virginia /F-6403-2013; Pitkin, Matthew/I-3802-2013; Vyatchanin, Sergey/J-2238-2012; van Putten, Maurice/F-5237-2011; Khalili, Farit/D-8113-2012; Chiadini, Francesco/E-1812-2015; Vecchio, Alberto/F-8310-2015; Mow-Lowry, Conor/F-8843-2015; Ottaway, David/J-5908-2015; Postiglione, Fabio/O-4744-2015; Messaritaki, Eirini/D-7393-2016; Sigg, Daniel/I-4308-2015; Pinto, Innocenzo/L-3520-2016; Kawazoe, Fumiko/F-7700-2011; Freise, Andreas/F-8892-2011; Kawabe, Keita/G-9840-2011; Tarallo, Marco/B-2096-2012; Finn, Lee Samuel/A-3452-2009; Agresti, Juri/G-8168-2012; 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; Zhao, Chunnong/C-2403-2013; Ju, Li/C-2623-2013 OI Chow, Jong/0000-0002-2414-5402; Frey, Raymond/0000-0003-0341-2636; Howell, Eric/0000-0001-7891-2817; LONGO, Maurizio/0000-0001-8325-4003; Pierro, Vincenzo/0000-0002-6020-5521; Ward, Robert/0000-0001-5503-5241; Whelan, John/0000-0001-5710-6576; Fairhurst, Stephen/0000-0001-8480-1961; Lueck, Harald/0000-0001-9350-4846; Lam, Ping Koy/0000-0002-4421-601X; Galdi, Vincenzo/0000-0002-4796-3600; Sylvestre, Julien/0000-0001-8136-4348; McClelland, David/0000-0001-6210-5842; Strain, Kenneth/0000-0002-2066-5355; Aulbert, Carsten/0000-0002-1481-8319; Messaritaki, Eirini/0000-0002-9917-4160; Freise, Andreas/0000-0001-6586-9901; MATTA, VINCENZO/0000-0002-2046-4027; MARANO, Stefano/0000-0002-5307-0980; Whiting, Bernard F/0000-0002-8501-8669; Veitch, John/0000-0002-6508-0713; Papa, M.Alessandra/0000-0002-1007-5298; Boschi, Valerio/0000-0001-8665-2293; Biswas, Rahul/0000-0002-0774-8906; Pinto, Innocenzo M./0000-0002-2679-4457; Stuver, Amber/0000-0003-0324-5735; Nishizawa, Atsushi/0000-0003-3562-0990; Zweizig, John/0000-0002-1521-3397; O'Shaughnessy, Richard/0000-0001-5832-8517; Pitkin, Matthew/0000-0003-4548-526X; Chiadini, Francesco/0000-0002-9339-8622; Vecchio, Alberto/0000-0002-6254-1617; Postiglione, Fabio/0000-0003-0628-3796; Sigg, Daniel/0000-0003-4606-6526; Tarallo, Marco/0000-0001-5169-4987; Finn, Lee Samuel/0000-0002-3937-0688; Agresti, Juri/0000-0001-6119-2470; Allen, Bruce/0000-0003-4285-6256; Zhao, Chunnong/0000-0001-5825-2401; NR 76 TC 50 Z9 50 U1 2 U2 13 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 MAR PY 2008 VL 77 IS 6 AR 062004 DI 10.1103/PhysRevD.77.062004 PG 22 WC Astronomy & Astrophysics; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA 282CF UT WOS:000254544500008 ER PT J AU Abbott, B Abbott, R Adhikari, R Agresti, J Ajith, P Allen, B Amin, R Anderson, SB Anderson, WG Arain, M Araya, M Armandula, H Ashley, M Aston, S Aufmuth, P Aulbert, C Babak, S Ballmer, S Bantilan, H Barish, BC Barker, C Barker, D Barr, B Barriga, P Barton, MA Bayer, K Belczynski, K Betzwieser, J Beyersdorf, PT Bhawal, B Bilenko, IA Billingsley, G Biswas, R Black, E Blackburn, K Blackburn, L Blair, D Bland, B Bogenstahl, J Bogue, L Bork, R Boschi, V Bose, S Brady, PR Braginsky, VB Brau, JE Brinkmann, M Brooks, A Brown, DA Bullington, A Bunkowski, A Buonanno, A Burmeister, O Busby, D Butler, WE Byer, RL Cadonati, L Cagnoli, G Camp, JB Cannizzo, J Cannon, K Cantley, CA Cao, J Cardenas, L Carter, K Casey, MM Castaldi, G Cepeda, C Chalkey, E Charlton, P Chatterji, S Chelkowski, S Chen, Y Chiadini, F Chin, D Chin, E Chow, J Christensen, N Clark, J Cochrane, P Cokelaer, T Colacino, CN Coldwell, R Conte, R Cook, D Corbitt, T Coward, D Coyne, D Creighton, JDE Creighton, TD Croce, RP Crooks, DRM Cruise, AM Cumming, A Dalrymple, J D'Ambrosio, E Danzmann, K Davies, G Debra, D Degallaix, J Degree, M Demma, T Dergachev, V Desai, S DeSalvo, R Dhurandhar, S Diaz, M Dickson, J Di Credico, A Diederichs, G Dietz, A Doomes, EE Drever, RWP Dumas, JC Dupuis, RJ Dwyer, JG Ehrens, P Espinoza, E Etzel, T Evans, M Evans, T Fairhurst, S Fan, Y Fazi, D Fejer, MM Finn, LS Fiumara, V Fotopoulos, N Franzen, A Franzen, KY Freise, A Frey, R Fricke, T Fritschel, P Frolov, VV Fyffe, M Galdi, V Ganezer, KS Garofoli, J Gholami, I Giaime, JA Giampanis, S Giardina, KD Goda, K Goetz, E Goggin, L Gonzalez, G Gossler, S Grant, A Gras, S Gray, C Gray, M Greenhalgh, J Gretarsson, AM Grosso, R Grote, H Grunewald, S Guenther, M Gustafson, R Hage, B Hammer, D Hanna, C Hanson, J Harms, J Harry, G Harstad, E Hayler, T Heefner, J Heng, IS Heptonstall, A Heurs, M Hewitson, M Hild, S Hirose, E Hoak, D Hosken, D Hough, J Howell, E Hoyland, D Huttner, SH Ingram, D Innerhofer, E Ito, M Itoh, Y Ivanov, A Jackrel, D Johnson, B Johnson, WW Jones, DI Jones, G Jones, R Ju, L Kalmus, P Kalogera, V Kasprzyk, D Katsavounidis, E Kawabe, K Kawamura, S Kawazoe, F Kells, W Keppel, DG Khalili, FY Kim, C King, P Kissel, JS Klimenko, S Kokeyama, K Kondrashov, V Kopparapu, RK Kozak, D Krishnan, B Kwee, P Lam, PK Landry, M Lantz, B Lazzarini, A Lee, B Lei, M Leiner, J Leonhardt, V Leonor, I Libbrecht, K Lindquist, P Lockerbie, NA Longo, M Lormand, M Lubinski, M Luck, H Machenschalk, B MacInnis, M Mageswaran, M Mailand, K Malec, M Mandic, V Marano, S Marka, S Markowitz, J Maros, E Martin, I Marx, JN Mason, K Matone, L Matta, V Mavalvala, N McCarthy, R McClelland, DE McGuire, SC McHugh, M McKenzie, K McNabb, JWC McWilliams, S Meier, T Melissinos, A Mendell, G Mercer, RA Meshkov, S Messaritaki, E Messenger, CJ Meyers, D Mikhailov, E Mitra, S Mitrofanov, VP Mitselmakher, G Mittleman, R Miyakawa, O Mohanty, S Moreno, G Mossavi, K MowLowry, C Moylan, A Mudge, D Mueller, G Mukherjee, S Muller-Ebhardt, H Munch, J Murray, P Myers, E Myers, J Nash, T Newton, G Nishizawa, A Nocera, F Numata, K O'Reilly, B O'Shaughnessy, R Ottaway, DJ Overmier, H Owen, BJ Pan, Y Papa, MA Parameshwaraiah, V Parameswariah, C Patel, P Pedraza, M Penn, S Pierro, V Pinto, IM Pitkin, M Pletsch, H Plissi, MV Postiglione, F Prix, R Quetschke, V Raab, F Rabeling, D Radkins, H Rahkola, R Rainer, N Rakhmanov, M Rawlins, K Ray-Majumder, S Re, V Regimbau, T Rehbein, H Reid, S Reitze, DH Ribichini, L 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 Sanders, GH Sannibale, V Saraf, S Sarin, P Sathyaprakash, BS Sato, S Saulson, PR Savage, R Savov, P Sazonov, A Schediwy, S 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 Sidles, JA Siemens, X Sigg, D Sinha, S Sintes, AM Slagmolen, BJJ Slutsky, J Smith, JR Smith, MR Somiya, K Strain, KA Strom, DM Stuver, A Summerscales, TZ Sun, KX Sung, M Sutton, PJ Takahashi, H Tanner, DB Tarallo, M 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 Ungarelli, C Urbanek, K Vahlbruch, H Vallisneri, M Van Den Broeck, C van Putten, M Varvella, M Vass, S Vecchio, A Veitch, J Veitch, P Villar, A Vorvick, C Vyachanin, SP Waldman, SJ Wallace, L Ward, H Ward, R Watts, K Webber, D Weidner, A Weinert, M Weinstein, A Weiss, R Wen, S Wette, K Whelan, JT Whitbeck, DM Whitcomb, SE Whiting, BF Wiley, S Wilkinson, C Willems, PA Williams, L Willke, B Wilmut, I Winkler, W Wipf, CC Wise, S Wiseman, AG Woan, G Woods, D Wooley, R Worden, J Wu, W Yakushin, I Yamamoto, H Yan, Z Yoshida, S Yunes, N Zanolin, M Zhang, J Zhang, L Zhao, C Zotov, N Zucker, M Muhlen, HZ Zweizig, J AF Abbott, B. Abbott, R. Adhikari, R. Agresti, J. Ajith, P. Allen, B. Amin, R. Anderson, S. B. Anderson, W. G. Arain, M. Araya, M. Armandula, H. Ashley, M. 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. Bayer, K. Belczynski, K. Betzwieser, J. Beyersdorf, P. T. Bhawal, B. Bilenko, I. A. Billingsley, G. Biswas, R. Black, E. Blackburn, K. Blackburn, L. Blair, D. Bland, B. Bogenstahl, J. Bogue, L. Bork, R. Boschi, V. Bose, S. Brady, P. R. Braginsky, V. B. Brau, J. E. Brinkmann, M. Brooks, A. Brown, D. A. Bullington, A. Bunkowski, A. Buonanno, A. Burmeister, O. Busby, D. Butler, W. E. Byer, R. L. Cadonati, L. Cagnoli, G. Camp, J. B. Cannizzo, J. Cannon, K. Cantley, C. A. Cao, J. Cardenas, L. Carter, K. Casey, M. M. Castaldi, G. Cepeda, C. Chalkey, E. Charlton, P. Chatterji, S. Chelkowski, S. Chen, Y. Chiadini, F. Chin, D. Chin, E. Chow, J. Christensen, N. Clark, J. Cochrane, P. Cokelaer, T. Colacino, C. N. Coldwell, R. Conte, R. Cook, D. Corbitt, T. Coward, D. Coyne, D. Creighton, J. D. E. Creighton, T. D. Croce, R. P. Crooks, D. R. M. Cruise, A. M. Cumming, A. Dalrymple, J. D'Ambrosio, E. Danzmann, K. Davies, G. DeBra, D. Degallaix, J. Degree, M. Demma, T. Dergachev, V. Desai, S. DeSalvo, R. Dhurandhar, S. Diaz, M. Dickson, J. Di Credico, A. Diederichs, G. Dietz, A. Doomes, E. E. Drever, R. W. P. Dumas, J. -C. Dupuis, R. J. Dwyer, J. G. Ehrens, P. Espinoza, E. Etzel, T. Evans, M. Evans, T. Fairhurst, S. Fan, Y. Fazi, D. Fejer, M. M. Finn, L. S. Fiumara, V. Fotopoulos, N. Franzen, A. Franzen, K. Y. Freise, A. Frey, R. Fricke, T. Fritschel, P. Frolov, V. V. Fyffe, M. Galdi, V. Ganezer, K. S. Garofoli, J. Gholami, I. Giaime, J. A. Giampanis, S. Giardina, K. D. Goda, K. Goetz, E. Goggin, L. Gonzalez, G. Gossler, S. Grant, A. Gras, S. Gray, C. Gray, M. Greenhalgh, J. Gretarsson, A. M. Grosso, R. Grote, H. Grunewald, S. Guenther, M. Gustafson, R. Hage, B. Hammer, D. Hanna, C. Hanson, J. Harms, J. Harry, G. Harstad, E. Hayler, T. Heefner, J. Heng, I. S. Heptonstall, A. Heurs, M. Hewitson, M. Hild, S. Hirose, E. Hoak, D. Hosken, D. Hough, J. Howell, E. Hoyland, D. Huttner, S. H. Ingram, D. Innerhofer, E. Ito, M. Itoh, Y. Ivanov, A. Jackrel, D. Johnson, B. Johnson, W. W. Jones, D. I. Jones, G. Jones, R. Ju, L. Kalmus, P. Kalogera, V. Kasprzyk, D. Katsavounidis, E. Kawabe, K. Kawamura, S. Kawazoe, F. Kells, W. Keppel, D. G. Khalili, F. Ya. Kim, C. King, P. Kissel, J. S. Klimenko, S. Kokeyama, K. Kondrashov, V. Kopparapu, R. K. Kozak, D. Krishnan, B. Kwee, P. Lam, P. K. Landry, M. Lantz, B. Lazzarini, A. Lee, B. Lei, M. Leiner, J. Leonhardt, V. Leonor, I. Libbrecht, K. Lindquist, P. Lockerbie, N. A. Longo, M. Lormand, M. Lubinski, M. Lueck, H. Machenschalk, B. MacInnis, M. Mageswaran, M. Mailand, K. Malec, M. Mandic, V. Marano, S. Marka, S. Markowitz, J. Maros, E. Martin, I. Marx, J. N. Mason, K. Matone, L. Matta, V. Mavalvala, N. McCarthy, R. McClelland, D. E. McGuire, S. C. McHugh, M. McKenzie, K. McNabb, J. W. C. McWilliams, S. Meier, T. Melissinos, A. Mendell, G. Mercer, R. A. Meshkov, S. Messaritaki, E. Messenger, C. J. Meyers, D. Mikhailov, E. Mitra, S. Mitrofanov, V. P. Mitselmakher, G. Mittleman, R. Miyakawa, O. Mohanty, S. Moreno, G. Mossavi, K. MowLowry, C. Moylan, A. Mudge, D. Mueller, G. Mukherjee, S. Muller-Ebhardt, H. Munch, J. Murray, P. Myers, E. Myers, J. Nash, T. Newton, G. Nishizawa, A. Nocera, F. Numata, K. O'Reilly, B. O'Shaughnessy, R. Ottaway, D. J. Overmier, H. Owen, B. J. Pan, Y. Papa, M. A. Parameshwaraiah, V. Parameswariah, C. Patel, P. Pedraza, M. Penn, S. Pierro, V. Pinto, I. M. Pitkin, M. Pletsch, H. Plissi, M. V. Postiglione, F. Prix, R. Quetschke, V. Raab, F. Rabeling, D. Radkins, H. Rahkola, R. Rainer, N. Rakhmanov, M. Rawlins, K. Ray-Majumder, S. Re, V. Regimbau, T. Rehbein, H. Reid, S. Reitze, D. H. Ribichini, L. 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. Sanders, G. H. Sannibale, V. Saraf, S. Sarin, P. Sathyaprakash, B. S. Sato, S. Saulson, P. R. Savage, R. Savov, P. Sazonov, A. Schediwy, S. 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. Sidles, J. A. Siemens, X. Sigg, D. Sinha, S. Sintes, A. M. Slagmolen, B. J. J. Slutsky, J. Smith, J. R. Smith, M. R. Somiya, K. Strain, K. A. Strom, D. M. Stuver, A. Summerscales, T. Z. Sun, K. -X. Sung, M. Sutton, P. J. Takahashi, H. Tanner, D. B. Tarallo, M. 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. Ungarelli, C. Urbanek, K. Vahlbruch, H. Vallisneri, M. Van Den Broeck, C. van Putten, M. Varvella, M. Vass, S. Vecchio, A. Veitch, J. Veitch, P. Villar, A. Vorvick, C. Vyachanin, S. P. Waldman, S. J. Wallace, L. Ward, H. Ward, R. Watts, K. Webber, D. Weidner, A. Weinert, M. Weinstein, A. Weiss, R. Wen, S. Wette, K. Whelan, J. T. Whitbeck, D. M. Whitcomb, S. E. Whiting, B. F. Wiley, S. Wilkinson, C. Willems, P. A. Williams, L. Willke, B. Wilmut, I. Winkler, W. Wipf, C. C. Wise, S. Wiseman, A. G. Woan, G. Woods, D. Wooley, R. Worden, J. Wu, W. Yakushin, I. Yamamoto, H. Yan, Z. Yoshida, S. Yunes, N. Zanolin, M. Zhang, J. Zhang, L. Zhao, C. Zotov, N. Zucker, M. Muehlen, H. zur Zweizig, J. TI Search for gravitational waves from binary inspirals in S3 and S4 LIGO data SO PHYSICAL REVIEW D LA English DT Article ID BLACK-HOLE BINARIES; GAMMA-RAY BURSTS; NEUTRON-STAR; COMPACT BINARIES; 2ND-POST-NEWTONIAN ORDER; CONSTRAINING POPULATION; SYNTHESIS MODELS; RATES; RADIATION; MERGERS AB We report on a search for gravitational waves from the coalescence of compact binaries during the third and fourth LIGO science runs. The search focused on gravitational waves generated during the inspiral phase of the binary evolution. In our analysis, we considered three categories of compact binary systems, ordered by mass: (i) primordial black hole binaries with masses in the range 0.35M center dot m(1), m(2) 1.0M center dot, (ii) binary neutron stars with masses in the range 1.0M center dot m(1), m(2) 3.0M center dot, and (iii) binary black holes with masses in the range 3.0M center dot m(1), m(2) m(max) with the additional constraint m(1) + m(2) m(max), where m(max) was set to 40.0M center dot and 80.0M center dot in the third and fourth science runs, respectively. Although the detectors could probe to distances as far as tens of Mpc, no gravitational-wave signals were identified in the 1364 hours of data we analyzed. Assuming a binary population with a Gaussian distribution around 0.75 - 0.75M center dot, 1.4 - 1.4M center dot, and 5.0 - 5.0M center dot, we derived 90%- confidence upper limit rates of 4.9 yr(-1)L(10)(-1) for primordial black hole binaries, 1.2 yr(-1)L(10)(-1) for binary neutron stars, and 0: 5 yr(-1)L(10)(-1) for stellar mass binary black holes, where L-10 is 10(10) times the blue-light luminosity of the Sun. C1 [Abbott, B.; Abbott, R.; Adhikari, R.; Agresti, J.; Anderson, S. B.; Araya, M.; Armandula, H.; Ballmer, S.; Barish, B. C.; Bhawal, B.; Billingsley, G.; Black, E.; Blackburn, K.; Bork, R.; Boschi, V.; Brown, D. A.; Busby, D.; Cardenas, L.; Cepeda, C.; Chatterji, S.; Creighton, T. D.; D'Ambrosio, E.; DeSalvo, R.; Drever, R. W. P.; Dupuis, R. J.; Ehrens, P.; Espinoza, E.; Etzel, T.; Evans, M.; Fairhurst, S.; Fazi, D.; Goggin, L.; 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.; Mandic, V.; Maros, E.; Marx, J. N.; Meshkov, S.; Messaritaki, E.; Meyers, D.; Miyakawa, O.; Muller-Ebhardt, H.; Nash, T.; Nocera, F.; Robertson, N. A.; Russell, P.; Samidi, M.; Sanders, G. H.; Sannibale, V.; Sears, B.; Siemens, X.; Smith, M. R.; Sutton, P. J.; Tarallo, M.; Traylor, G.; Tyler, W.; Varvella, M.; Vass, S.; Villar, A.; Waldman, S. J.; Wallace, L.; Ward, R.; Webber, D.; Weinstein, A.; Whitcomb, S. E.; Willems, P. A.; Yamamoto, H.; Zhang, L.; Zweizig, J.] CALTECH, LIGO, Pasadena, CA 91125 USA. [Aulbert, C.; Babak, S.; Chen, Y.; Gholami, I.; Grunewald, S.; Krishnan, B.; Machenschalk, B.; Papa, M. A.; Prix, R.; 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. [Ajith, P.; Allen, B.; Brinkmann, M.; Bunkowski, A.; Burmeister, O.; Chelkowski, S.; Cochrane, P.; Danzmann, K.; Grote, H.; Harms, J.; Heurs, M.; Hewitson, M.; Lueck, H.; Mossavi, K.; Pletsch, H.; Rainer, N.; Rehbein, H.; Ribichini, L.; Ruediger, A.; Schilling, R.; Schnabel, R.; Seifert, F.; Smith, J. R.; Somiya, K.; Weidner, A.; 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. [Ashley, M.; Chow, J.; Dickson, J.; Gossler, S.; Gray, M.; Lam, P. K.; McClelland, D. E.; McKenzie, K.; MowLowry, C.; Moylan, A.; Rabeling, D.; Scott, S. M.; Searle, A. C.; Slagmolen, B. J. J.; Wette, K.] Australian Natl Univ, Canberra, ACT 0200, Australia. [Garofoli, J.; Wiley, S.] Calif State Univ Dominguez Hills, Carson, CA 90747 USA. [Brown, D. A.; Savov, P.; Siemens, X.; Thorne, K. S.; Vallisneri, M.] CALTECH, CaRT, Pasadena, CA 91125 USA. [Cokelaer, T.; Davies, G.; Dietz, A.; Fairhurst, S.; Jones, G.; Regimbau, T.; Robinson, C.; Romano, J. D.; Sathyaprakash, B. S.; Schutz, B. F.; Sengupta, A. S.; Van Den Broeck, C.] Cardiff Univ, Cardiff CF2 3YB, Wales. [Bantilan, H.; Christensen, N.] Carleton Coll, Northfield, MN 55057 USA. [Charlton, P.; Matone, L.] Charles Sturt Univ, Wagga Wagga, NSW 2678, Australia. [Dwyer, J. G.; Kalmus, P.; Marka, S.; Rollins, J.] Columbia Univ, New York, NY 10027 USA. [Gretarsson, A. M.] Embry Riddle Aeronaut Univ, Prescott, AZ 86301 USA. [Penn, S.] Hobart & William Smith Coll, Geneva, NY 14456 USA. [Dhurandhar, S.; Mitra, S.] Inter Univ Ctr Astron & Astrophys, Pune 411007, Maharashtra, India. [Barker, C.; Barker, D.; Bland, B.; Cook, D.; 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 99352 USA. [Bogue, L.; Carter, K.; Evans, T.; Frolov, V. V.; Fyffe, M.; Giaime, J. A.; Giardina, K. D.; Hanson, J.; Hoak, D.; Lormand, M.; O'Reilly, B.; Overmier, H.; Parameswariah, C.; Patel, P.; Pedraza, M.; Riesen, R.; Roddy, S.; Romie, J.; Sellers, D.; Sibley, A.; Thacker, J.; Traylor, G.; Watts, K.; Wooley, R.; Yakushin, I.] LIGO Livingston Observ, Livingston, LA 70754 USA. [Bayer, K.; Blackburn, L.; Cadonati, L.; Cao, J.; Corbitt, T.; Fritschel, P.; Goda, K.; Harry, G.; Innerhofer, E.; Katsavounidis, E.; MacInnis, M.; Markowitz, J.; Mason, K.; Mavalvala, N.; Mikhailov, E.; Mittleman, R.; Ottaway, D. J.; Rawlins, K.; Ruet, L.; Sarin, P.; Shoemaker, D. H.; van Putten, M.; Wen, S.; Wipf, C. C.; Zanolin, M.; Zucker, M.] MIT, LIGO, Cambridge, MA 02139 USA. [Amin, R.; Betzwieser, J.; Giaime, J. A.; Gonzalez, G.; Hanna, C.; Johnson, W. W.; Kopparapu, R. K.; Rodriguez, A.; Slutsky, J.; Sung, M.] Louisiana State Univ, Baton Rouge, LA 70803 USA. [Amin, R.; Zotov, N.] Louisiana Tech Univ, Ruston, LA 71272 USA. [McHugh, M.] Loyola Univ, New Orleans, LA 70118 USA. [Bilenko, I. A.; Braginsky, V. B.; Khalili, F. Ya.; Mitrofanov, V. P.; Vyachanin, S. P.] Moscow MV Lomonosov State Univ, Moscow 119992, Russia. [Camp, J. B.; Cannizzo, J.; McWilliams, S.; Numata, K.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Kawamura, S.; Kawazoe, F.; Kokeyama, K.; Leonhardt, V.; Nishizawa, A.; Sakata, S.; Sato, S.] Natl Astron Observ, Tokyo 1818588, Japan. [Belczynski, K.; Kalogera, V.; Kim, C.; O'Shaughnessy, R.] Northwestern Univ, Evanston, IL 60208 USA. [Saraf, S.] Rochester Inst Technol, Rochester, NY 14623 USA. [Greenhalgh, J.; Hayler, T.; Wilmut, I.] Rutherford Appleton Lab, Didcot OX11 0QX, Oxon, England. [Beyersdorf, P. T.] San Jose State Univ, San Jose, CA 95192 USA. [Yoshida, S.] SE Louisiana Univ, Hammond, LA 70402 USA. [Doomes, E. E.; McGuire, S. C.] So Univ & A&M Coll, Baton Rouge, LA 70813 USA. [Bullington, A.; Byer, R. L.; DeBra, D.; Di Credico, A.; Fejer, M. M.; Jackrel, D.; Lantz, B.; Route, R.; Sinha, S.; Sun, K. -X.; Urbanek, K.] Stanford Univ, Stanford, CA 94305 USA. [Dalrymple, J.; Di Credico, A.; Hirose, E.; Saulson, P. R.] Syracuse Univ, Syracuse, NY 13244 USA. [Desai, S.; Finn, L. S.; McNabb, J. W. C.; Owen, B. J.; Rakhmanov, M.; Stuver, A.; Thorne, K. A.; Whitbeck, D. M.; Yunes, N.] Penn State Univ, University Pk, PA 16802 USA. [Diaz, M.; Grosso, R.; Mohanty, S.; Mukherjee, S.; Torres, C.] 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. [Aufmuth, P.; Danzmann, K.; Diederichs, G.; Franzen, A.; Hage, B.; Hild, S.; Kwee, P.; Lueck, H.; Malec, M.; Meier, T.; Thuering, A.; Vahlbruch, H.; Willke, B.; Muehlen, H. zur] Leibniz Univ Hannover, D-30167 Hannover, Germany. [Brooks, A.; Hosken, D.; Mudge, D.; Munch, J.; Veitch, P.] Univ Adelaide, Adelaide, SA 5005, Australia. [Aston, S.; Colacino, C. N.; Cruise, A. M.; Freise, A.; Hoyland, D.; Kasprzyk, D.; Re, V.; Robinson, E. L.; Ungarelli, C.; Vecchio, A.] Univ Birmingham, Birmingham B15 2TT, W Midlands, England. [Arain, M.; Coldwell, R.; Franzen, K. Y.; Klimenko, S.; Mercer, R. A.; Mitselmakher, G.; Mueller, G.; Quetschke, V.; Reitze, D. H.; Sazonov, A.; Tanner, D. B.; Whiting, B. F.; Williams, L.; Wise, S.; Wu, W.] Univ Florida, Gainesville, FL 32611 USA. [Barriga, P.; Barton, M. A.; Bogenstahl, J.; Cagnoli, G.; Cantley, C. A.; Casey, M. M.; Chalkey, E.; Clark, J.; Crooks, D. R. M.; Cumming, A.; Grant, A.; Heng, I. S.; Heptonstall, A.; Hough, J.; Huttner, S. H.; Jones, R.; Martin, I.; Messenger, C. J.; Murray, P.; Newton, G.; Reid, S.; Robertson, N. A.; Rowan, S.; Strain, K. A.; Taylor, R.; Tokmakov, K. V.; Torrie, C.; Veitch, J.; Ward, H.; Woan, G.] Univ Glasgow, Glasgow G12 8QQ, Lanark, Scotland. [Buonanno, A.; Pan, Y.; Pitkin, M.; Plissi, M. V.; Shawhan, P.] Univ Maryland, College Pk, MD 20742 USA. [Chin, D.; Dergachev, V.; Goetz, E.; Gustafson, R.; Riles, K.; Zhang, J.] Univ Michigan, Ann Arbor, MI 48109 USA. [Brau, J. E.; Frey, R.; Fricke, T.; Harstad, E.; Ito, M.; Leonor, I.; Rahkola, R.; Schofield, R.; Strom, D. M.] Univ Oregon, Eugene, OR 97403 USA. [Butler, W. E.; Giampanis, S.; Melissinos, A.] Univ Rochester, Rochester, NY 14627 USA. [Chiadini, F.; Conte, R.; Fiumara, V.; Longo, M.; Marano, S.; Matta, V.; Postiglione, F.] Univ Salerno, I-84084 Salerno, Italy. [Castaldi, G.; Croce, R. P.; Demma, T.; Galdi, V.; Pierro, V.; Pinto, I. M.] Univ Sannio, I-82100 Benevento, Italy. [Jones, D. I.] Univ Southampton, Southampton SO17 1BJ, Hants, England. [Lockerbie, N. A.] Univ Strathclyde, Glasgow G1 1XQ, Lanark, Scotland. [Siemens, X.] Univ Washington, Seattle, WA 98195 USA. [Barton, M. A.; Blair, D.; Chin, E.; Degallaix, J.; Dumas, J. -C.; Fan, Y.; Gras, S.; Howell, E.; Ju, L.; Lee, B.; Schediwy, S.; Yan, Z.; Zhao, C.] Univ Western Australia, Crawley, WA 6009, Australia. [Anderson, W. G.; Biswas, R.; Brady, P. R.; Cannon, K.; Creighton, J. D. E.; Fotopoulos, N.; Hammer, D.; Itoh, Y.; Papa, M. A.; Ray-Majumder, S.; Wiseman, A. G.; Woods, D.] Univ Wisconsin, Milwaukee, WI 53201 USA. Vassar Coll, New York, NY 12604 USA. [Bose, S.; Leiner, J.; Rogan, A. M.] Washington State Univ, Pullman, WA 99164 USA. RP Abbott, B (reprint author), CALTECH, LIGO, Pasadena, CA 91125 USA. RI Khalili, Farit/D-8113-2012; Chiadini, Francesco/E-1812-2015; Vecchio, Alberto/F-8310-2015; Mow-Lowry, Conor/F-8843-2015; Ottaway, David/J-5908-2015; Postiglione, Fabio/O-4744-2015; Messaritaki, Eirini/D-7393-2016; Tarallo, Marco/B-2096-2012; Sigg, Daniel/I-4308-2015; Pinto, Innocenzo/L-3520-2016; Harms, Jan/J-4359-2012; Chow, Jong/A-3183-2008; Frey, Raymond/E-2830-2016; Chen, Yanbei/A-2604-2013; Allen, Bruce/K-2327-2012; Bilenko, Igor/D-5172-2012; Strain, Kenneth/D-5236-2011; Raab, Frederick/E-2222-2011; Casey, Morag/C-9703-2010; Mitrofanov, Valery/D-8501-2012; Martin, Iain/A-2445-2010; Hild, Stefan/A-3864-2010; McClelland, David/E-6765-2010; Pitkin, Matthew/I-3802-2013; Schutz, Bernard/B-1504-2010; Rowan, Sheila/E-3032-2010; Agresti, Juri/G-8168-2012; Zhao, Chunnong/C-2403-2013; Ju, Li/C-2623-2013; Re, Virginia /F-6403-2013; Barker, David/A-5671-2013; Lueck, Harald/F-7100-2011; Kawabe, Keita/G-9840-2011; Kawazoe, Fumiko/F-7700-2011; Freise, Andreas/F-8892-2011; Galdi, Vincenzo/B-1670-2008; Lam, Ping Koy/A-5276-2008; Finn, Lee Samuel/A-3452-2009; Vyatchanin, Sergey/J-2238-2012; Howell, Eric/H-5072-2014; Ward, Robert/I-8032-2014; OI Chiadini, Francesco/0000-0002-9339-8622; Vecchio, Alberto/0000-0002-6254-1617; Postiglione, Fabio/0000-0003-0628-3796; Tarallo, Marco/0000-0001-5169-4987; Sigg, Daniel/0000-0003-4606-6526; Chow, Jong/0000-0002-2414-5402; Frey, Raymond/0000-0003-0341-2636; Allen, Bruce/0000-0003-4285-6256; Strain, Kenneth/0000-0002-2066-5355; McClelland, David/0000-0001-6210-5842; Pitkin, Matthew/0000-0003-4548-526X; Agresti, Juri/0000-0001-6119-2470; Zhao, Chunnong/0000-0001-5825-2401; Lueck, Harald/0000-0001-9350-4846; Galdi, Vincenzo/0000-0002-4796-3600; Lam, Ping Koy/0000-0002-4421-601X; Finn, Lee Samuel/0000-0002-3937-0688; Freise, Andreas/0000-0001-6586-9901; MATTA, VINCENZO/0000-0002-2046-4027; MARANO, Stefano/0000-0002-5307-0980; Whiting, Bernard F/0000-0002-8501-8669; Veitch, John/0000-0002-6508-0713; Papa, M.Alessandra/0000-0002-1007-5298; Stuver, Amber/0000-0003-0324-5735; 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; Howell, Eric/0000-0001-7891-2817; LONGO, Maurizio/0000-0001-8325-4003; Pierro, Vincenzo/0000-0002-6020-5521; Ward, Robert/0000-0001-5503-5241; Whelan, John/0000-0001-5710-6576; Fairhurst, Stephen/0000-0001-8480-1961; Boschi, Valerio/0000-0001-8665-2293; Pinto, Innocenzo M./0000-0002-2679-4457 NR 56 TC 100 Z9 100 U1 3 U2 18 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 MAR PY 2008 VL 77 IS 6 AR 062002 DI 10.1103/PhysRevD.77.062002 PG 13 WC Astronomy & Astrophysics; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA 282CF UT WOS:000254544500006 ER PT J AU Rubinstein, R Luo, LS AF Rubinstein, Robert Luo, Li-Shi TI Theory of the lattice Boltzmann equation: Symmetry properties of discrete velocity sets SO PHYSICAL REVIEW E LA English DT Article ID NONIDEAL GASES; MODELS; DIMENSIONS AB The lattice Boltzmann equation replaces continuous particle velocity space by a finite set; the velocity distribution function then varies over a finite-dimensional vector space instead of over an infinite-dimensional function space. The number of linearly independent moments of the distribution function in a lattice Boltzmann model cannot exceed the number of velocities; finite dimensionality therefore necessarily induces linear dependences among the moments that do not exist in a continuous theory. Given a finite velocity set, it is important to know which moments are free of these dependences. Elementary group theory is applied to the solution of this problem. It is found that decomposing the velocity set into subsets that transform among themselves under an appropriate symmetry group makes it straightforward to uncover linear dependences among the moments. The construction of some standard two- and three-dimensional models is reviewed from this viewpoint, and procedures for constructing higher-dimensional models are suggested. C1 [Rubinstein, Robert] NASA, Langley Res Ctr, Hampton, VA 23681 USA. [Luo, Li-Shi] Old Dominion Univ, Dept Math & Stat, Ctr Computat Sci, Norfolk, VA 23529 USA. RP Rubinstein, R (reprint author), NASA, Langley Res Ctr, Hampton, VA 23681 USA. EM r.rubinstein@nasa.gov; lluo@odu.edu RI Luo, Li-Shi/A-4561-2011 OI Luo, Li-Shi/0000-0003-1215-7892 NR 35 TC 24 Z9 24 U1 0 U2 7 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 1539-3755 J9 PHYS REV E JI Phys. Rev. E PD MAR PY 2008 VL 77 IS 3 AR 036709 DI 10.1103/PhysRevE.77.036709 PN 2 PG 11 WC Physics, Fluids & Plasmas; Physics, Mathematical SC Physics GA 282AL UT WOS:000254539900113 PM 18517559 ER PT J AU Gamero-Castano, M AF Gamero-Castano, Manuel TI Characterization of the electrosprays of 1-ethyl-3-methylimidazolium bis(trifluoromethylsulfonyl) imide in vacuum SO PHYSICS OF FLUIDS LA English DT Article ID UNIVERSAL SCALING LAWS; TAYLOR CONES; IONIC LIQUIDS; JETS; SURFACES; BREAKUP; MODEL AB The electrosprays of 1-ethyl-3-methylimidazolium bis(trifluoromethylsulfonyl) imide are composed of a complex mixture of ions and charged droplets, which can be analyzed to determine the structure of the beam and infer significant features of the electrohydrodynamic atomization. In particular, we use a combination of retarding potential and time of flight techniques to study these beams and are able to quantify the voltage drop along the cone jet, together with the velocity and diameter of the jet at the breakup location, confirm the strong influence of viscosity and electrification in the breakup, show that the electric field in and near the Taylor cone tip is insensitive to external electrostatic parameters, and study the spatial distribution of ions and droplets, whereby the paradoxical absence of ions in the outmost region of the beam is established. The research described in this article can be exploited in the modeling of capillary instability of charged jets: testing the results of these models is difficult, especially when nanojets are involved, and our findings and techniques provide the experimental support required by the theoretical activity. The present research is also applicable to the modeling of colloid thruster beams. (C) 2008 American Institute of Physics. C1 Univ Calif Irvine, Dept Mech & Aerosp Engn, Irvine, CA 92717 USA. Jet Propuls Lab, Pasadena, CA 91108 USA. RP Gamero-Castano, M (reprint author), Univ Calif Irvine, Dept Mech & Aerosp Engn, Irvine, CA 92717 USA. NR 29 TC 11 Z9 11 U1 2 U2 5 PU AMER INST PHYSICS PI MELVILLE PA CIRCULATION & FULFILLMENT DIV, 2 HUNTINGTON QUADRANGLE, STE 1 N O 1, MELVILLE, NY 11747-4501 USA SN 1070-6631 J9 PHYS FLUIDS JI Phys. Fluids PD MAR PY 2008 VL 20 IS 3 AR 032103 DI 10.1063/1.2899658 PG 11 WC Mechanics; Physics, Fluids & Plasmas SC Mechanics; Physics GA 281ZO UT WOS:000254537600009 ER PT J AU Birn, J Borovsky, JE Hesse, M AF Birn, J. Borovsky, J. E. Hesse, M. TI Properties of asymmetric magnetic reconnection SO PHYSICS OF PLASMAS LA English DT Article ID CHALLENGE; MAGNETOTAIL; MHD AB Properties of magnetic reconnection are investigated in two-dimensional, resistive magnetohydrodynamic (MHD) simulations of current sheets separating plasmas with different magnetic field strengths and densities. Specific emphasis is on the influence of the external parameters on the reconnection rate. The effect of the dissipation in the resistive MHD model is separated from this influence by evaluating resistivity dependence together with the dependence on the background parameters. Two scenarios are considered, which may be distinguished as driven and nondriven reconnection. In either scenario, the maximum reconnection rate (electric field) is found to depend on appropriate hybrid expressions based on a magnetic field strength and an Alfven speed derived from the characteristic values in the two inflow regions. The scaling compares favorably with an analytic formula derived recently by Cassak and Shay [Phys. Plasmas 14, 102114 (2007)] applied to the regime of fast reconnection. An investigation of the energy flow and conversion in the vicinity of the reconnection site revealed a significant role of enthalpy flux generation, in addition to the expected conversion of Poynting flux to kinetic energy flux. This enthalpy flux generation results from Ohmic heating as well as adiabatic, that is, compressional heating. The latter is found more important when the magnetic field strengths in the two inflow regions are comparable in magnitude. (C) 2008 American Institute of Physics. C1 [Birn, J.; Borovsky, J. E.] Los Alamos Natl Lab, Los Alamos, NM 87545 USA. [Hesse, M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Birn, J (reprint author), Los Alamos Natl Lab, POB 1663, Los Alamos, NM 87545 USA. EM jbirn@lanl.gov RI Hesse, Michael/D-2031-2012; NASA MMS, Science Team/J-5393-2013 OI NASA MMS, Science Team/0000-0002-9504-5214 NR 15 TC 43 Z9 43 U1 0 U2 1 PU AMER INST PHYSICS PI MELVILLE PA CIRCULATION & FULFILLMENT DIV, 2 HUNTINGTON QUADRANGLE, STE 1 N O 1, MELVILLE, NY 11747-4501 USA SN 1070-664X J9 PHYS PLASMAS JI Phys. Plasmas PD MAR PY 2008 VL 15 IS 3 AR 032101 DI 10.1063/1.2888491 PG 13 WC Physics, Fluids & Plasmas SC Physics GA 281ZR UT WOS:000254537900005 ER PT J AU Peters, GH Smith, JA Mungas, GS Bearman, GH Shiraishi, L Beegle, LW AF Peters, Gregory H. Smith, J. Anthony Mungas, Gregory S. Bearman, Gregory H. Shiraishi, Lori Beegle, Luther W. TI RASP-based sample acquisition of analogue Martian permafrost samples: Implications for NASA's Phoenix scout mission SO PLANETARY AND SPACE SCIENCE LA English DT Article DE Mars geological processes; Mars sampling technology : Mars in situ investigations ID GROUND ICE; MARS; BEHAVIOR AB Sample acquisition studies of ice-dirt mixtures under simulated Martian conditions approximating the 2007/8 Phoenix Scout mission are reported. The experiments were performed using a prototype rapid acquisition sampling package (RASP) that is similar to the one mounted on the 2007/8 Phoenix scout robotic arm. This mission will acquire a sample from permafrost-like regolith that is estimated at strengths near 45 MPa to measure the volatile composition including H(2)O. Sublimation loss during sample acquisition and transfer will have a significant effect on the determination of water content, a major Phoenix mission goal. Laboratory sample acquisition was performed under Martian ambient pressures (5 Torr) in which water is unstable and ice quickly sublimates. Basalt samples consisting of various size, and shapes subjected to various temperature ranges were used as the aggregate material of the water saturated permafrost analogues expected to be found at the Phoenix landing site. In our laboratory experiments roughly 5-6% of the initial water-ice was sublimed due to energy imparted by the tool to the sample during sample acquisition. This loss is in addition to any others from passive sublimation as the samples are transferred to the instruments for analysis. We determined that the energy necessary to excavate the permafrost samples with the RASP to be on the order of 0.05 W h/cm(3). Finally, we discuss the potential to use a RASP on future in situ Martian missions. (c) 2007 Elsevier Ltd. All rights reserved. C1 [Beegle, Luther W.] CALTECH, Jet Prop Lab, Planetary Sci Sect, Pasadena, CA 91109 USA. [Shiraishi, Lori] CALTECH, Jet Prop Lab, Instrument Mech Engn Sect, Pasadena, CA 91109 USA. [Peters, Gregory H.; Smith, J. Anthony; Mungas, Gregory S.; Bearman, Gregory H.] CALTECH, Jet Prop Lab, In Situ Instrument Syst Sect, Pasadena, CA 91109 USA. RP Beegle, LW (reprint author), CALTECH, Jet Prop Lab, Planetary Sci Sect, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM Gregory.H.Peters@jpl.nasa.gov; J.Anthony.Smith@jpl.nasa.gov; Greg.S.Mungas@jpl.nasa.gov; Gregory.H.Bearman@jpl.nasa.gov; Lori.R.Shiraishi@jpl.nasa.gov; Luther.Beegle@jpl.nasa.gov RI Beegle, Luther/A-6354-2010 NR 12 TC 4 Z9 4 U1 2 U2 6 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0032-0633 J9 PLANET SPACE SCI JI Planet Space Sci. PD MAR PY 2008 VL 56 IS 3-4 BP 303 EP 309 DI 10.1016/j.pss.2007.10.001 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 279QZ UT WOS:000254371000001 ER PT J AU Graves, SDB Mckay, CP Griffith, CA Ferri, F Fulchignoni, M AF Graves, S. D. B. McKay, C. P. Griffith, C. A. Ferri, F. Fulchignoni, M. TI Rain and hail can reach the surface of Titan SO PLANETARY AND SPACE SCIENCE LA English DT Article DE Titan; methane; Huygens; rain; hail ID HUYGENS PROBE; ATMOSPHERE; METHANE; CLOUDS; CONDENSATION; EVAPORATION; DESCENT; ETHANE; VAPOR; LAKES AB We have calculated the condensation and evaporation of ternary CH4-N-2-C2H6 liquid drops and solid CH4 hail as they fall through Titan's lower atmosphere to determine the likelihood that precipitation reaches the ground. Assuming the humidity profile determined by the Huygens probe, binary liquid CH4/N-2 condensate grows in the region from similar to 8 to 15 km in Titan's atmosphere because the combined humidity of CH4 and N-2 exceeds saturation. These drops evaporate below similar to 8 km. We determine the fate of 10 mu m seeds composed of ethane, which is expected to provide condensation sites. In addition, we study the fate of already formed raindrops with radii of 1-4.75 mm falling out of the growth region. High (50%) and low (0%) ethane relative humidities (RH) are considered in the calculation. We find that drops with radii similar to 3 mm and smaller dropping from 8 km reach the ground in compositional equilibrium with the atmosphere in the high ethane RH case as a result of the stabilizing influence of the ethane, and evaporate in the atmosphere in the low ethane RH case. Large drops (> similar to 3 mm) reach the surface large and cold because the latent heat loss due to the evaporation of methane cools the drop and slows the evaporation rate. Pure methane hail hits the ground if its radius is initially more than 4 mm at 16 km above the surface and sublimates in the atmosphere if its radius is smaller. (c) 2007 Elsevier Ltd. All rights reserved. C1 [Graves, S. D. B.; McKay, C. P.] NASA, Ames Res Ctr, Div Space Sci, Moffett Field, CA 94035 USA. [Griffith, C. A.] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA. [Fulchignoni, M.] Observ Paris, Lab Etud Spatiales & Instrumentat Astrophys, F-92195 Meudon, France. [Ferri, F.] Univ Padua, I-35131 Padua, Italy. RP Graves, SDB (reprint author), CALTECH, Dept Planetary Sci, MS 150-21, Pasadena, CA 91125 USA. EM sdgraves@gps.caltech.edu NR 31 TC 53 Z9 54 U1 0 U2 6 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0032-0633 J9 PLANET SPACE SCI JI Planet Space Sci. PD MAR PY 2008 VL 56 IS 3-4 BP 346 EP 357 DI 10.1016/j.pss.2007.11.001 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 279QZ UT WOS:000254371000005 ER PT J AU Furfaro, R Dohm, JM Fink, W Kargel, J Schulze-Makuch, D Fairen, AG Palmero-Rodriguez, A Baker, VR Ferre, PT Hare, TM Tarbell, MA Miyamoto, H Komatsu, G AF Furfaro, R. Dohm, J. M. Fink, W. Kargel, J. Schulze-Makuch, D. Fairen, A. G. Palmero-Rodriguez, A. Baker, V. R. Ferre, P. T. Hare, T. M. Tarbell, M. A. Miyamoto, H. Komatsu, G. TI The search for life beyond Earth through fuzzy expert systems SO PLANETARY AND SPACE SCIENCE LA English DT Article DE fuzzy logic; tier-scalable mission autonomy; astrobiology; search for life; bobotic planetary exploration; autonomous planetary reconnaissance ID PLANETARY RECONNAISSANCE MISSIONS; LINGUISTIC-SYNTHESIS; GLOBAL DISTRIBUTION; PARADIGM SHIFT; THARSIS REGION; MARS ODYSSEY; ENVIRONMENTS; EXPLORATION; ENCELADUS; DEPOSITS AB Autonomy will play a key role in future science-driven, tier-scalable robotic planetary reconnaissance to extremely challenging (by existing means), locales on Mars and elsewhere that have the potential to yield significant geological and possibly exobiologic information. The full-scale and optimal deployment of the agents employed by tier-scalable architectures requires the design, implementation, and integration of an intelligent reconnaissance system. Such a system should be designed to enable fully automated and comprehensive characterization of an operational area, as well as to integrate existing information with acquired, "in transit" spatial and temporal sensor data, to identify and home in on prime candidate locales. These may include locales with the greatest potential of containing life. Founded on the premise that water and energy are key to life, we have designed a fuzzy system that can (1) acquire the appropriate past/present water/energy indicators while the tier-scalable mission architecture is deployed (first layer), and (2) evaluate habitability through a specialized fuzzy knowledge-base of the water and energy information (second layer) acquired in (1). The system has been tested through hypothetical deployments at two hypothesized regions on Mars. The fuzzy-based expert's simulation results corroborate the same conclusions provided by the human expert, and thus highlight the system's potential capability to effectively and autonomously reason as an interdisciplinary scientist in the quest for life. While the approach is demonstrated for Mars, the methodology is general enough to be extended to other planetary bodies. It can be readily modified and updated as our interdisciplinary understanding of planetary environments improves. We believe this work represents a foundational step toward implementing higher-level intelligence in robotic. tier-scalable planetary reconnaissance within and beyond the solar system. (c) 2007 Elsevier Ltd. All rights reserved. C1 [Furfaro, R.] Univ Arizona, Dept Aerosp & Mech Engn, Tucson, AZ 85721 USA. [Dohm, J. M.; Kargel, J.; Baker, V. R.; Ferre, P. T.] Univ Arizona, Dept Hydrol & Water Resources, Tucson, AZ 85721 USA. [Dohm, J. M.; Baker, V. R.] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA. [Fink, W.; Tarbell, M. A.] CALTECH, Visual & Autonomous Explorat Syst Res Lab, Div Phys Math & Astron, Pasadena, CA 91125 USA. [Schulze-Makuch, D.] Washington State Univ, Dept Geol, Pullman, WA 99164 USA. [Fairen, A. G.] NASA, Ames Res Ctr, Space Sci & Astrobiol Div, Moffett Field, CA 94035 USA. [Hare, T. M.] US Geol Survey, Flagstaff, AZ 86001 USA. [Palmero-Rodriguez, A.] Univ Tokyo, Dept Earth & Planetary Sci, Tokyo 1130033, Japan. [Miyamoto, H.] Univ Tokyo, Dept Geosyst Engn, Tokyo, Japan. [Komatsu, G.] Univ Annunzio, Int Res Sch Planetary Sci, Pescara, Italy. RP Furfaro, R (reprint author), Univ Arizona, Dept Aerosp & Mech Engn, Tucson, AZ 85721 USA. EM robertof@email.arizona.edu RI Miyamoto, Hideaki/B-9666-2008; Miyamoto, Hideaki/E-3381-2012; Dohm, James/A-3831-2014; Komatsu, Goro/I-7822-2012; OI Komatsu, Goro/0000-0003-4155-108X; Hare, Trent/0000-0001-8842-389X; Schulze-Makuch, Dirk/0000-0002-1923-9746 NR 64 TC 14 Z9 14 U1 0 U2 4 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 MAR PY 2008 VL 56 IS 3-4 BP 448 EP 472 DI 10.1016/j.pss.2007.09.006 PG 25 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 279QZ UT WOS:000254371000015 ER PT J AU Oberst, J Schwarz, G Behnke, T Hoffmann, H Matz, KD Flohrer, J Hirsch, H Roatsch, T Scholten, F Hauber, E Brinkmann, B Jaumann, R Williams, D Kirk, R Duxbury, T Leu, C Neukum, G AF Oberst, J. Schwarz, G. Behnke, T. Hoffmann, H. Matz, K. -D. Flohrer, J. Hirsch, H. Roatsch, T. Scholten, F. Hauber, E. Brinkmann, B. Jaumann, R. Williams, D. Kirk, R. Duxbury, T. Leu, C. Neukum, G. TI The imaging performance of the SRC on Mars Express SO PLANETARY AND SPACE SCIENCE LA English DT Article DE Mars; Mars express; instruments; cameras ID RESOLUTION STEREO CAMERA; MARTIAN ATMOSPHERE; VERTICAL STRUCTURE; CHRONOLOGY; HRSC AB The Mars Express spacecraft carries the pushbroom scanner high-resolution stereo camera (HRSC) and its added imaging subsystem super resolution channel (SRC). The SRC is equipped with its own optical system and a 1024 x 1024 framing sensor. SRC produces snapshots with 2.3 in ground pixel size from the nominal spacecraft pericenter height of 250 km, which are typically embedded in the central part of the large HRSC scenes. The salient features of the SRC are its light-weight optics, a reliable CCD detector, and high-speed read-out electronics. The quality and effective visibility of details in the SRC images unfortunately falls short of what has been expected. in cases where thermal balance cannot be reached, artifacts, Such as blurring and "ghost features" are observed in the images. In addition, images show large numbers of blemish pixels and are plagued by electronic noise. As a consequence, we have developed various image improving algorithms, which are discussed in this paper. While results are encouraging, further studies of image restoration by dedicated processing appear worthwhile. The SRC has obtained more than 6940 images at the time of writing (1 September 2007), which often show fascinating details in surface morphology. SRC images are highly useful for a variety of applications in planetary geology, for studies of the Mars atmosphere, and for astrometric observations of the Martian satellites. This paper will give a full account of the design philosophy, technical concept, calibration, operation, integration with HRSC, and performance, as well as science accomplishments of the SRC. (c) 2007 Elsevier Ltd. All rights reserved. C1 [Oberst, J.; Behnke, T.; Hoffmann, H.; Matz, K. -D.; Flohrer, J.; Hirsch, H.; Roatsch, T.; Scholten, F.; Hauber, E.; Brinkmann, B.; Jaumann, R.] German Aerosp Ctr, Inst Planetary Res, D-12489 Berlin, Germany. [Schwarz, G.] German Aerosp Ctr, Remote Sensing Technol Inst, Oberpfaffenhofen, Germany. [Williams, D.] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85287 USA. [Kirk, R.] US Geol Survey, Flagstaff, AZ 86001 USA. [Duxbury, T.] Jet Propuls Lab, Pasadena, CA USA. [Leu, C.; Neukum, G.] Free Univ Berlin, Inst Geosci, D-1000 Berlin, Germany. RP Oberst, J (reprint author), German Aerosp Ctr, Inst Planetary Res, Rutherfordstr 2, D-12489 Berlin, Germany. EM Juergen.Oberst@dlr.de NR 29 TC 20 Z9 21 U1 1 U2 5 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 MAR PY 2008 VL 56 IS 3-4 BP 473 EP 491 DI 10.1016/j.pss.2007.09.009 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 279QZ UT WOS:000254371000016 ER PT J AU Hawes, WM Duffey, MR AF Hawes, W. Michael Duffey, Michael R. TI Formulation of Financial Valuation Methodologies for NASA's Human Spaceflight Projects SO PROJECT MANAGEMENT JOURNAL LA English DT Article DE NASA; real options; project valuation AB The National Aeronautics and Space Administration (NASA) must continually evaluate proposals to upgrade its human spaceflight systems. These proposals may be initiated to enhance safety, improve performance, or provide improved cost value. In the current restrictive budget environment, the cost valuation should be strengthened to ensure the best use of limited funding. NASA has not frequently utilized financial analysis in project consideration, and business case analysis is often lacking during annual budgetary assessments. Some of the reasons inhibiting financial analysis are uncertainty in the projections of long life-cycle costs, gains that may seem intangible and difficult to monetize, and the political environment. This paper explores ways in which some financial valuation methods, coupled with reformulation of project cash flows, might enhance NASA's analysis process. Among these methods is real option analysis (ROA), which is discussed in the context of several NASA upgrade projects. C1 [Hawes, W. Michael] NASA Headquarters, Space Operat Mission Directorate, Washington, DC USA. [Duffey, Michael R.] George Washington Univ, Dept Engn Management & Syst Engn, Washington, DC USA. RP Hawes, WM (reprint author), NASA Headquarters, Space Operat Mission Directorate, Washington, DC USA. NR 17 TC 5 Z9 5 U1 0 U2 2 PU WILEY PERIODICALS, INC PI MALDEN PA COMMERCE PLACE, 350 MAIN STREET, MALDEN, MA 02148-529 USA SN 8756-9728 J9 PROJ MANAG J JI Proj. Manag. J. PD MAR PY 2008 VL 39 IS 1 BP 85 EP 94 DI 10.1002/pmj.20032 PG 10 WC Management SC Business & Economics GA V18OM UT WOS:000208014100008 ER PT J AU Almimi, AA Kulahci, M Montgomery, DC AF Almimi, Ashraf A. Kulahci, Murat Montgomery, Douglas C. TI Estimation of missing observations in two-level split-plot designs SO QUALITY AND RELIABILITY ENGINEERING INTERNATIONAL LA English DT Article DE missing observations; half-normal plot; unreplicated two-level factorial and fractional factorial split-plot designs; alias chains of effects AB Inserting estimates for the missing observations from split-plot designs restores their balanced or orthogonal structure and alleviates the difficulties in the statistical analysis. In this article, we extend a method due to Draper and Stoneman to estimate the missing observations from unreplicated two-level factorial and fractional factorial split-plot (FSP and FFSP) designs. The missing observations, which can either be from the same whole plot, from different whole plots, or comprise entire whole plots, are estimated by equating to zero a number of specific contrast columns equal to the number of the missing observations. These estimates are inserted into the design table and the estimates for the remaining effects (or alias chains of effects as the case with FFSP designs) are plotted on two half-normal plots: one for the whole-plot effects and the other for the subplot effects. If the smaller effects do not point at the origin, then different contrast columns to some or all of the initial ones should be discarded and the plots re-examined for bias. Using examples, we show how the method provides estimates for the missing observations that are very close to their actual values. Copyright (C) 2007 John Wiley & Sons, Ltd. C1 [Almimi, Ashraf A.; Kulahci, Murat; Montgomery, Douglas C.] Arizona State Univ, Dept Ind Engn, Tempe, AZ 85287 USA. [Kulahci, Murat] Tech Univ Denmark, DK-2800 Lyngby, Denmark. [Almimi, Ashraf A.] NASA, Langley Res Ctr, Hampton, VA 23681 USA. RP Montgomery, DC (reprint author), Arizona State Univ, Dept Ind Engn, Tempe, AZ 85287 USA. EM doug.montgomery@asu.edu OI kulahci, murat/0000-0003-4222-9631 NR 11 TC 0 Z9 0 U1 1 U2 3 PU JOHN WILEY & SONS LTD PI CHICHESTER PA THE ATRIUM, SOUTHERN GATE, CHICHESTER PO19 8SQ, W SUSSEX, ENGLAND SN 0748-8017 J9 QUAL RELIAB ENG INT JI Qual. Reliab. Eng. Int. PD MAR PY 2008 VL 24 IS 2 BP 127 EP 152 DI 10.1002/qre.871 PG 26 WC Engineering, Multidisciplinary; Engineering, Industrial; Operations Research & Management Science SC Engineering; Operations Research & Management Science GA 280GP UT WOS:000254414100002 ER PT J AU Muller, J Kylander, M Wust, RAJ Weiss, D Martinez-Cortizas, A LeGrande, AN Jennerjahn, T Behling, H Anderson, WT Jacobson, G AF Muller, Joanne Kylander, Malin Wuest, Raphael A. J. Weiss, Dominik Martinez-Cortizas, Antonio LeGrande, Allegra N. Jennerjahn, Tim Behling, Herman Anderson, William T. Jacobson, Geraldine TI Possible evidence for wet Heinrich phases in tropical NE Australia: the Lynch's Crater deposit SO QUATERNARY SCIENCE REVIEWS LA English DT Article ID ABRUPT CLIMATE-CHANGE; INTERDECADAL PACIFIC OSCILLATION; NORTHEASTERN BRAZIL; CONVERGENCE ZONE; ICE; EVENTS; CYCLES; RECORD; OCEAN; CONSEQUENCES AB Unarguably, one of the most significant paleoclimatological discoveries of the last two decades has been that of abrupt climate events (Dansgaard-Oeschger cycles and Heinrich events). Most evidence for these events has originated from the high-latitude Northern Hemisphere.. with few records documenting the response of the low latitude Southern Hemisphere. Here we present new data from Lynch's Crater, a unique terrestrial record from NE-Australia that may show evidence for southward propagations of the Intertropical Convergence Zone (ITCZ) during abrupt climate perturbations as a result of alteration of the low latitude air masses. Proxies for precipitation/wetness indicate enhanced rainfall in the region during Heinrich events (H events 1-3) and the 8.2 ka Northern Hemisphere cold event. A fully coupled atmosphere/ocean climate model simulating a 1 Sv freshwater influx to the North Atlantic Ocean produces a scenario which agrees with the climate changes shown by the Lynch's Crater record. The model shows precipitation anomalies that include a southward migration of the ITCZ and a zonal shift in mid-latitude storm tracks over the Southern Hemisphere equatorial region. These data indicate large-scale shifts of the austral summer ITCZ position that is known to control monsoonal precipitation in NE Australia. This terrestrial record from Australia may demonstrate the involvement of the tropical western Pacific Ocean in ITCZ migrations during abrupt climate events of the last glacial period. Defining such past migrations offers insight into the importance and role of the equatorial region in global climate dynamics. (C) 2007 Elsevier Ltd. All rights reserved. C1 [Muller, Joanne] Woods Hole Oceanog Inst, Woods Hole, MA 02543 USA. [Kylander, Malin; Weiss, Dominik] James Cook Univ N Queensland, Sch Earth Sci, Townsville, Qld 4811, Australia. [Kylander, Malin; Weiss, Dominik] Nat Hist Museum London, London SW7 2AZ, England. [Martinez-Cortizas, Antonio] Fac Biol, Dept Edafol & Quim Agricola, E-15782 Santiago, Spain. [LeGrande, Allegra N.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA. [LeGrande, Allegra N.] Columbia Univ, Ctr Climate Syst Res, New York, NY 10025 USA. [Jennerjahn, Tim] Zentrum Marine Tropenokol, D-28359 Bremen, Germany. [Behling, Herman] Univ Gottingen, Albrecht Von Haller Inst Plant Sci, Dept Palynol & Climate Dynam, D-37073 Gottingen, Germany. [Anderson, William T.] Florida Int Univ, SE Environm Res Ctr, Dept Earth Sci, Miami, FL 33199 USA. [Jacobson, Geraldine] Australian Nucl Sci & Technol Org, Sydney, NSW, Australia. RP Muller, J (reprint author), Woods Hole Oceanog Inst, Mail Stop 21, Woods Hole, MA 02543 USA. EM jmuller@whoi.edu RI LeGrande, Allegra/D-8920-2012; Martinez Cortizas, Antonio/M-6196-2015; OI LeGrande, Allegra/0000-0002-5295-0062; Martinez Cortizas, Antonio/0000-0003-0430-5760; Weiss, Dominik/0000-0001-8074-9430 NR 42 TC 49 Z9 51 U1 0 U2 12 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0277-3791 J9 QUATERNARY SCI REV JI Quat. Sci. Rev. PD MAR PY 2008 VL 27 IS 5-6 BP 468 EP 475 DI 10.1016/j.quascirev.2007.11.006 PG 8 WC Geography, Physical; Geosciences, Multidisciplinary SC Physical Geography; Geology GA 293RH UT WOS:000255351900004 ER PT J AU Adams, DO Yarger, CB Webb, NJ Hunter, A Oborn, KD Saether, E Wilson, JW Badavi, FF AF Adams, D. O. Yarger, C. B. Webb, N. J. Hunter, A. Oborn, K. D. Saether, E. Wilson, J. W. Badavi, F. F. TI Multi-functional sandwich composite for spacecraft applications SO SAMPE JOURNAL LA English DT Article AB Multi-functional sandwich composites are proposed to integrate the previously separate objectives of radiation shielding, structural integrity, damage tolerance, thermal insulation, and debris/micrometeoroid shielding into a viable structural design. Effective radiation shielding is provided through the selection of hydrogen-rich polymeric materials for the primary sandwich composite structure. Using facesheet and core materials selected based on radiation shielding simulations, prototype sandwich configurations were manufactured that featured transverse reinforcements for damage tolerance and an internal Surlyn(R) self-healing membrane layer. Flatwise tensile and core shear testing were performed to assess material compatibility between the facesheet and core layers and to identify any manufacturing-related problems. Acceptable interlaminar strengths were obtained for all configurations investigated. The results from this initial assessment suggest that multi-functional sandwich composite configurations may be used to maximize the efficiency of advanced material usage in future structural spacecraft applications. C1 [Adams, D. O.; Yarger, C. B.; Webb, N. J.; Hunter, A.; Oborn, K. D.] Univ Utah, Dept Mech Engn, Salt Lake City, UT 84112 USA. [Saether, E.; Wilson, J. W.] NASA Langley Res Ctr, Hampton, VA USA. [Badavi, F. F.] Christopher Newport Univ, Dept Phys, Newport News, VA 23606 USA. RP Adams, DO (reprint author), Univ Utah, Dept Mech Engn, Salt Lake City, UT 84112 USA. NR 11 TC 1 Z9 1 U1 1 U2 7 PU SAMPE PUBLISHERS PI COVINA PA 1161 PARKVIEW DRIVE, COVINA, CA 91722 USA SN 0091-1062 J9 SAMPE J JI Sampe J. PD MAR-APR PY 2008 VL 44 IS 2 BP 38 EP 49 PG 12 WC Engineering, Multidisciplinary; Materials Science, Multidisciplinary SC Engineering; Materials Science GA 266UT UT WOS:000253463300005 ER PT J AU Zander, R Mahieu, E Demoulin, P Duchatelet, P Roland, G Servais, C De Maziere, M Reimann, S Rinsland, CP AF Zander, R. Mahieu, E. Demoulin, P. Duchatelet, P. Roland, G. Servais, C. De Maziere, M. Reimann, S. Rinsland, C. P. TI Our changing atmosphere: Evidence based on long-term infrared solar observations at the Jungfraujoch since 1950 SO SCIENCE OF THE TOTAL ENVIRONMENT LA English DT Article; Proceedings Paper CT International Conference Celebrating the 75th Anniversary of the High Altitude Research Station Jungfraujoch CY SEP 11-13, 2006 CL Interlaken, SWITZERLAND DE atmospheric composition changes; infrared remote sensing; infrared spectroscopy; climate change; Montreal and Kyoto Protocols ID GROUND-BASED FTIR; SPECTROSCOPIC MEASUREMENTS; STRATOSPHERIC CHLORINE; COLUMN ABUNDANCES; STATION; NORTHERN; TREND; HEMISPHERE; SPECTRA; CLONO2 AB The Institute of Astrophysics of the University of Liege has been present at the High Altitude Research Station Jungfraujoch, Switzerland, since the late 1940s, to perform spectrometric solar observations under dry and weakly polluted high-mountain conditions. Several solar atlases of photometric quality, extending altogether from the near-ultra-violet to the middle-infrared, were produced between 1956 and 1994, first with grating spectrometers then with Fourier transform instruments. During the early 1970s, scientific concerns emerged about atmospheric composition changes likely to set in as a consequence of the growing usage of nitrogen-containing agricultural fertilisers and the industrial production of chlorine-bearing compounds such as the chlorofluorocarbons and hydrochlorofluorocarbons. Resulting releases to the atmosphere with ensuing photolysis in the stratosphere and catalytic depletion of the protective ozone layer prompted a worldwide consortium of chemical manufacturing companies to solicit the Liege group to help in clarifying these concerns by undertaking specific observations with its existing Jungfraujoch instrumentation. The following pages evoke the main steps that led from quasi full sun-oriented studies to priority investigations of the Earth's atmosphere, in support of both the Montreal and the Kyoto Protocols. (c) 2007 Elsevier B.V. All rights reserved. C1 [Zander, R.; Mahieu, E.; Demoulin, P.; Duchatelet, P.; Roland, G.; Servais, C.] Univ Liege, Inst Astrophys & Geophys, B-4000 Liege, Belgium. [De Maziere, M.] Belgian Inst Space Aeron, Brussels, Belgium. [Rinsland, C. P.] NASA, Langley Res Ctr, Hampton, VA 23665 USA. RP Zander, R (reprint author), Univ Liege, Inst Astrophys & Geophys, 17,Allee 6 Aout, B-4000 Liege, Belgium. EM r.zander@ulg.ac.be RI Reimann, Stefan/A-2327-2009; OI Reimann, Stefan/0000-0002-9885-7138; Mahieu, Emmanuel/0000-0002-5251-0286 NR 52 TC 40 Z9 41 U1 1 U2 8 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0048-9697 EI 1879-1026 J9 SCI TOTAL ENVIRON JI Sci. Total Environ. PD MAR 1 PY 2008 VL 391 IS 2-3 BP 184 EP 195 DI 10.1016/j.scitotenv.2007.10.018 PG 12 WC Environmental Sciences SC Environmental Sciences & Ecology GA 261FU UT WOS:000253065300003 PM 18067951 ER PT J AU Fong, R AF Fong, Ron TI Goodbye to LD50? SO SCIENTIST LA English DT Letter C1 NASA, Moffett Field, CA 94035 USA. RP Fong, R (reprint author), NASA, Moffett Field, CA 94035 USA. EM ronald.c.fong@nasa.gov NR 1 TC 0 Z9 0 U1 0 U2 0 PU SCIENTIST INC PI PHILADELPHIA PA 3535 MARKET ST, SUITE 200, PHILADELPHIA, PA 19104-3385 USA SN 0890-3670 J9 SCIENTIST JI Scientist PD MAR PY 2008 VL 22 IS 3 BP 16 EP 17 PG 2 WC Information Science & Library Science; Multidisciplinary Sciences SC Information Science & Library Science; Science & Technology - Other Topics GA 265IL UT WOS:000253352200010 ER PT J AU Michalek, G Gopalswamy, N Yashiro, S AF Michalek, G. Gopalswamy, N. Yashiro, S. TI Space weather application using projected velocity asymmetry of halo CMEs SO SOLAR PHYSICS LA English DT Article DE Sun : solar activity; Sun : coronal mass ejections ID CORONAL MASS EJECTIONS; CONE MODEL; STORMS AB Halo coronal mass ejections (HCMEs) originating from regions close to the center of the Sun are likely to be responsible for severe geomagnetic storms. It is important to predict geoeffectiveness of HCMEs by using observations when they are still near the Sun. Unfortunately, coronagraphic observations do not provide true speeds of CMEs because of projection effects. In the present paper, we present a new technique to allow estimates of the space speed and approximate source location using projected speeds measured at different position angles for a given HCME (velocity asymmetry). We apply this technique to HCMEs observed during 2001-2002 and find that the improved speeds are better correlated with the travel times of HCMEs to Earth and with the magnitudes of ensuing geomagnetic storms. C1 [Michalek, G.] Jagiellonian Univ, Astron Observ, Krakow, Poland. [Gopalswamy, N.] NASA, Goddard Space Flight Ctr, Solar Syst Explorat Div, Greenbelt, MD 20771 USA. [Yashiro, S.] Catholic Univ Amer, Ctr Solar & Space Weather, Washington, DC 20064 USA. RP Michalek, G (reprint author), Jagiellonian Univ, Astron Observ, Krakow, Poland. EM michalek@oa.uj.edu.pl RI Gopalswamy, Nat/D-3659-2012 NR 29 TC 6 Z9 6 U1 0 U2 1 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0038-0938 J9 SOL PHYS JI Sol. Phys. PD MAR PY 2008 VL 248 IS 1 BP 113 EP 123 DI 10.1007/s11207-008-9126-7 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 280QM UT WOS:000254441300008 ER PT J AU Lepping, RP Wu, CC Gopalswamy, N Berdichevsky, DB AF Lepping, R. P. Wu, C. -C. Gopalswamy, N. Berdichevsky, D. B. TI Average thickness of magnetosheath upstream of magnetic clouds at 1 AU versus solar longitude of source SO SOLAR PHYSICS LA English DT Article DE magnetic clouds; solar wind; shock waves; magnetosheath ID CORONAL MASS EJECTIONS; MAGNETOSPHERE; ORIGIN; FIELDS; SHOCK; WIND AB Starting with a large number (N = 100) of Wind magnetic clouds (MCs) and applying necessary restrictions, we find a proper set of N = 29 to investigate the average ecliptic plane projection of the upstream magnetosheath thickness as a function of the longitude of the solar source of the MCs, for those cases of MCs having upstream shock waves. A few of the obvious restrictions on the full set of MCs are the need for there to exist a driven upstream shock wave, knowledge of the MC's solar source, and restriction to only MCs of low axial latitudes. The analysis required splitting this set into two subsets according to average magnetosheath speed: slow/average (300-500 km s(-1)) and fast (500-1100 km s(-1)) speeds. Only the fast set gives plausible results, where the estimated magnetosheath thickness (Delta S) goes from 0.042 to 0.079 AU (at 1 AU) over the longitude sector of 0 degrees (adjusted source-center longitude of the average magnetic cloud) to 40 off center ( East or West), based on N = 11 appropriate cases. These estimates are well determined with a sigma (sigma) for the fit of 0.0055 AU, where s is effectively the same as root(chi- squared) for the appropriate quadratic fit. The associated linear correlation coefficient for Delta S versus vertical bar Longitude vertical bar was very good (c.c. = 0.93) for the fast range, and Delta S at 60 degrees longitude is extrapolated to be 2.7 times the value at 0 degrees. For the slower speeds we obtain the surprising result that Delta S is typically more-or-less constant at 0.040 +/- 0.013 AU at all longitudes, indicating that the MC as a driver, when moving close to the normal solar wind speed, has little influence on magnetosheath thickness. In some cases, the correct choice between two candidate solarsource longitudes for a fast MC might be made by noting the value of the observed Delta S just upstream of the MC. Also, we point out that, for the 29 events, the average sheath speed was well correlated with the quantity Delta V[= (< V-MC > - < V-UPSTREAM >)], and also with both < V-MC > and < V-MC,V-T > , where < V-MC > is the first one-hour average of the MC speed, < V-MC,V-T > is the average MC speed across the full MC, and < V-UPSTREAM > is a five-hour average of the solar wind speed just upstream of the shock. C1 [Lepping, R. P.] NASA, Goddard Space Flight Ctr, Space Weather Lab, Greenbelt, MD 20771 USA. [Wu, C. -C.] Univ Alabama, Huntsville, AL 35899 USA. [Gopalswamy, N.] NASA, Goddard Space Flight Ctr, Solar Syst Explorat Div, Greenbelt, MD 20771 USA. [Berdichevsky, D. B.] Sigma Space Corp, Lanham, MD 20706 USA. RP Lepping, RP (reprint author), NASA, Goddard Space Flight Ctr, Space Weather Lab, Greenbelt, MD 20771 USA. EM ronald.p.lepping@nasa.gov RI Gopalswamy, Nat/D-3659-2012 NR 30 TC 3 Z9 3 U1 0 U2 2 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0038-0938 EI 1573-093X J9 SOL PHYS JI Sol. Phys. PD MAR PY 2008 VL 248 IS 1 BP 125 EP 139 DI 10.1007/s11207-007-9111-6 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 280QM UT WOS:000254441300009 ER PT J AU Mckay, CP AF Mckay, Christopher P. TI An approach to searching for life on Mars, Europa, and Enceladus SO SPACE SCIENCE REVIEWS LA English DT Review DE life; Mars; Europa; Enceladus; second genesis ID GLOBAL DISTRIBUTION AB Near-term missions may be able to access samples of organic material from Mars, Europa, and Enceladus. The challenge for astrobiology will be to determine if this material is the remains of dead microorganisms or merely abiotic organic material. The remains of life that shares a common origin with life on Earth will be straightforward to detect using sophisticated methods such as DNA amplification. These methods are extremely sensitive but specific to Earth-like life. Detecting the remains of alien life-that does not have a genetic or biochemical commonality with Earth life-will be much more difficult. There is a general property of life that can be used to determine if organic material is of biological origin. This general property is the repeated use of a few specific organic molecules for the construction of biopolymers. For example, Earth-like life uses 20 amino acids to construct proteins, 5 nucleotide bases to construct DNA and RNA, and a few sugars to construct polysaccharides. This selectivity will result in a statistically anomalous distribution of organic molecules distinct from organic material of non-biological origin. Such a distinctive pattern, different from the pattern of Earth-like life, will be persuasive evidence for a second genesis of life. C1 NASA, Ames Res Ctr, Div Space Sci, Moffett Field, CA 94035 USA. RP Mckay, CP (reprint author), NASA, Ames Res Ctr, Div Space Sci, Mail Stop 245 3, Moffett Field, CA 94035 USA. EM cmckay@mail.arc.nasa.gov NR 15 TC 7 Z9 7 U1 2 U2 24 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0038-6308 J9 SPACE SCI REV JI Space Sci. Rev. PD MAR PY 2008 VL 135 IS 1-4 BP 49 EP 54 DI 10.1007/s11214-007-9229-8 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 322OB UT WOS:000257384100006 ER PT J AU Mahaffy, P AF Mahaffy, Paul TI Exploration of the habitability of Mars: Development of analytical protocols for measurement of organic carbon on the 2009 Mars science laboratory SO SPACE SCIENCE REVIEWS LA English DT Review DE Mars; organics; Mars Science Laboratory; Sample Analysis at Mars; investigation; astrobiology ID MARTIAN METEORITE ALH84001; POLYCYCLIC AROMATIC-HYDROCARBONS; CHROMATOGRAPHY-MASS-SPECTROMETRY; IN-SITU ANALYSES; AMINO-ACIDS; ATMOSPHERE; SURFACE; SEARCH; METHANE; ORIGIN AB The mission goal of the 2009 Mars Science Laboratory is to assess the habitability of a region on Mars. This large rover incorporates an Analytical Laboratory that contributes to this mission objective by means of a detailed characterization of mineralogy and chemistry. The Sample Analysis at Mars instrument suite in the Analytical Laboratory provides the capability to analyze volatiles released from rocks and soils and gases directly sample from the atmosphere. A primary focus of this suite is the detection and identification of organic molecules. The protocols for the extraction and analysis of organics under development for this mission are described as are experiments carried out on Mars analog samples to evaluate these methods. C1 NASA, Goddard Space Flight Ctr, Atmospher Expt Lab, Greenbelt, MD 20771 USA. RP Mahaffy, P (reprint author), NASA, Goddard Space Flight Ctr, Atmospher Expt Lab, Greenbelt, MD 20771 USA. EM Paul.R.Mahaffy@nasa.gov RI Mahaffy, Paul/E-4609-2012 NR 48 TC 31 Z9 31 U1 0 U2 7 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0038-6308 J9 SPACE SCI REV JI Space Sci. Rev. PD MAR PY 2008 VL 135 IS 1-4 BP 255 EP 268 DI 10.1007/s11214-007-9223-1 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 322OB UT WOS:000257384100018 ER PT J AU Bada, JL Ehrenfreund, P Grunthaner, F Blaney, D Coleman, M Farrington, A Yen, A Mathies, R Amudson, R Quinn, R Zent, A Ride, S Barron, L Botta, O Clark, B Glavin, D Hofmann, B Josset, JL Rettberg, P Robert, F Sephton, M AF Bada, J. L. Ehrenfreund, P. Grunthaner, F. Blaney, D. Coleman, M. Farrington, A. Yen, A. Mathies, R. Amudson, R. Quinn, R. Zent, A. Ride, S. Barron, L. Botta, O. Clark, B. Glavin, D. Hofmann, B. Josset, J. L. Rettberg, P. Robert, F. Sephton, M. TI Urey: Mars Organic and Oxidant Detector SO SPACE SCIENCE REVIEWS LA English DT Review DE Mars; life detection instrumentation; space research ID ATACAMA DESERT; MARTIAN SOIL; AMINO-ACIDS; LIFE; ATMOSPHERE; PRESERVATION; REACTIVITY; MOLECULES; METHANE; SEARCH AB One of the fundamental challenges facing the scientific community as we enter this new century of Mars research is to understand, in a rigorous manner, the biotic potential both past and present of this outermost terrestrial-like planet in our solar system. Urey: Mars Organic and Oxidant Detector has been selected for the Pasteur payload of the European Space Agency's (ESA's) ExoMars rover mission and is considered a fundamental instrument to achieve the mission's scientific objectives. The instrument is named Urey in recognition of Harold Clayton Urey's seminal contributions to cosmochemistry, geochemistry, and the study of the origin of life. The overall goal of Urey is to search for organic compounds directly in the regolith of Mars and to assess their origin. Urey will perform a groundbreaking investigation of the Martian environment that will involve searching for organic compounds indicative of life and prebiotic chemistry at a sensitivity many orders of magnitude greater than Viking or other in situ organic detection systems. Urey will perform the first in situ search for key classes of organic molecules using state-of-the-art analytical methods that provide part-per-trillion sensitivity. It will ascertain whether any of these molecules are abiotic or biotic in origin and will evaluate the survival potential of organic compounds in the environment using state-of-the-art chemoresistor oxidant sensors. C1 [Bada, J. L.] Univ Calif San Diego, Scripps Inst Oceanog, La Jolla, CA 92093 USA. [Ehrenfreund, P.] Leiden Univ, Leiden Inst Chem, NL-2300 RA Leiden, Netherlands. [Grunthaner, F.; Blaney, D.; Coleman, M.; Farrington, A.; Yen, A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Mathies, R.; Amudson, R.] Univ Calif Berkeley, Berkeley, CA 94720 USA. [Quinn, R.] NASA, Ames Res Ctr, SETI Inst, Moffett Field, CA 94035 USA. [Ride, S.] Imaginary Lines Inc, San Diego, CA 92122 USA. [Barron, L.] Univ Glasgow, Dept Chem, Glasgow G12 8QQ, Lanark, Scotland. [Botta, O.] Int Space Sci Inst, CH-3012 Bern, Switzerland. [Clark, B.] Lockheed Martin, Space Explorat Syst, Denver, CO 80201 USA. [Glavin, D.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Hofmann, B.] Nat Hist Museum Burgergemeinde Bern, CH-3005 Bern, Switzerland. [Josset, J. L.] Space Explorat Inst SPACE X, Neuchatel, Switzerland. [Rettberg, P.] Inst Aerosp Med Radiat Biol, D-51147 Cologne, Germany. [Robert, F.] Museum Natl Hist Nat, LEME NanoAnal, F-75005 Paris, France. [Sephton, M.] Univ London Imperial Coll Sci Technol & Med, Dept Earth Sci & Engn, London SW7 2AZ, England. RP Bada, JL (reprint author), Univ Calif San Diego, Scripps Inst Oceanog, La Jolla, CA 92093 USA. EM jbada@ucsd.edu RI Glavin, Daniel/D-6194-2012; Rettberg, Petra/K-2378-2015; OI Glavin, Daniel/0000-0001-7779-7765; Rettberg, Petra/0000-0003-4439-2395; Sephton, Mark/0000-0002-2190-5402 NR 36 TC 10 Z9 10 U1 4 U2 19 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0038-6308 J9 SPACE SCI REV JI Space Sci. Rev. PD MAR PY 2008 VL 135 IS 1-4 BP 269 EP 279 DI 10.1007/s11214-007-9213-3 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 322OB UT WOS:000257384100019 ER PT J AU Briggs, C Little, P AF Briggs, Clark Little, Patrick TI Impacts of organizational culture and personality traits on decision-making in technical organizations SO SYSTEMS ENGINEERING LA English DT Article DE organizational culture; decision making; decision analysis AB Technical organizations in industries such as aerospace or automotive regularly make major decisions regarding software and other tools to support mission-critical activities. These decisions take place at the enterprise level where functional departments must work together in ways not common before. Usually, these are high-impact, tension-filled decision activities that have long term effects. The organization needs a successful decision that stands the test of implementation and a sustained period of effective operation. The processes used in such cases generally follow analytical decision methods aimed at maximizing objectives. Understanding the characteristics of the organization, including the culture and the affected parties, in addition to the technical aspects of the decision may significantly increase the likelihood of success. (C) 2007 Wiley Periodicals, Inc. C1 [Briggs, Clark] CALTECH, Jet Prop Lab, NASA, Pasadena, CA 91109 USA. [Little, Patrick] Harvey Mudd Coll, Claremont, CA 91711 USA. RP Briggs, C (reprint author), CALTECH, Jet Prop Lab, NASA, M-S 158-224,4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM Clark.Briggs@jpl.nasa.gov FU National Aeronautics and Space Administration FX The research described in this paper was carried out in part at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. NR 23 TC 3 Z9 3 U1 1 U2 4 PU JOHN WILEY & SONS INC PI HOBOKEN PA 111 RIVER ST, HOBOKEN, NJ 07030 USA SN 1098-1241 J9 SYST ENG JI Syst. Eng. PD SPR PY 2008 VL 11 IS 1 BP 15 EP 26 DI 10.1002/sys.20083 PG 12 WC Engineering, Industrial; Operations Research & Management Science SC Engineering; Operations Research & Management Science GA 340RN UT WOS:000258662800002 ER PT J AU Weidman, PD Davis, AMJ Kubitschek, DG AF Weidman, P. D. Davis, A. M. J. Kubitschek, D. G. TI Crocco variable formulation for uniform shear flow over a stretching surface with transpiration: Multiple solutions and stability SO ZEITSCHRIFT FUR ANGEWANDTE MATHEMATIK UND PHYSIK LA English DT Article DE shear flow; boundary layer; plate stretching; suction; multiple solutions; stability ID BOUNDARY-LAYER FLOW; REVERSE FLOW; MOVING-WALL AB The simultaneous effects of transpiration through and tangential movement of a semi-infinite flat plate on the self-similar boundary layer flow driven by uniform shear in the far field is considered. Difficulties with standard shooting techniques are overcome using Crocco variables which also serve to better elucidate the solution structure. The stabilities of dual, triple and even quadruple steady flow solutions encountered in different ranges of plate stretching and wall stress are determined using a linear temporal stability analysis for the self-similar flow. C1 [Weidman, P. D.] Univ Colorado, Dept Mech Engn, Boulder, CO 80309 USA. [Davis, A. M. J.] Univ Alabama, Dept Math, Tuscaloosa, AL 35487 USA. [Kubitschek, D. G.] CALTECH, Jet Prop Lab, Opt Navigat Grp, Pasadena, CA 91109 USA. RP Weidman, PD (reprint author), Univ Colorado, Dept Mech Engn, Boulder, CO 80309 USA. NR 16 TC 10 Z9 10 U1 0 U2 1 PU BIRKHAUSER VERLAG AG PI BASEL PA VIADUKSTRASSE 40-44, PO BOX 133, CH-4010 BASEL, SWITZERLAND SN 0044-2275 J9 Z ANGEW MATH PHYS JI Z. Angew. Math. Phys. PD MAR PY 2008 VL 59 IS 2 BP 313 EP 332 DI 10.1007/s00033-006-6018-2 PG 20 WC Mathematics, Applied SC Mathematics GA 269XN UT WOS:000253684200007 ER PT J AU Choi, Y Wang, YH Yang, Q Cunnold, D Zeng, T Shim, C Luo, M Eldering, A Bucsela, E Gleason, J AF Choi, Yunsoo Wang, Yuhang Yang, Qing Cunnold, Derek Zeng, Tao Shim, Changsub Luo, Ming Eldering, Annmarie Bucsela, Eric Gleason, James TI Spring to summer northward migration of high O-3 over the western North Atlantic SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID ART.; TRANSPORT; TROPOSPHERE; POLLUTION; OZONE; MODEL AB Tropospheric O-3 columns retrieved from OMI and MLS measurements, NO2 columns from OMI, and upper tropospheric O-3 concentrations from TES over North America and the western North Atlantic from April to August 2005 are analyzed using the Regional chEmical and trAnsport Model (REAM). Large enhancements of column and upper tropospheric O-3 over the western North Atlantic comparable to those over the eastern United States are found in the satellite measurements and REAM simulations. The O-3 enhancement region migrates northward from spring to summer. Model analysis indicates that the northward migration is driven by seasonal shifts of O-3 transported from the stratosphere and that produced through photochemistry from surface emissions and lightning NOx. As their uncertainties improve, satellite measurements of O-3 and its precursors will be able to provide more quantitative constraints on pollutant outflow from the continents. C1 [Shim, Changsub; Luo, Ming; Eldering, Annmarie] Jet Prop Lab, Pasadena, CA 91109 USA. [Choi, Yunsoo; Wang, Yuhang; Yang, Qing; Cunnold, Derek; Zeng, Tao] Georgia Inst Technol, Dept Earth & Atmospher Sci, Atlanta, GA 30332 USA. [Bucsela, Eric; Gleason, James] NASA GSFC, Greenbelt, MD 20771 USA. RP Choi, Y (reprint author), Jet Prop Lab, Pasadena, CA 91109 USA. EM yunsoo.choi@jpl.nasa.gov RI Yang, Qing/H-3275-2011; Gleason, James/E-1421-2012; Wang, Yuhang/B-5578-2014 OI Yang, Qing/0000-0003-2067-5999; NR 18 TC 23 Z9 23 U1 0 U2 2 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 FEB 29 PY 2008 VL 35 IS 4 AR L04818 DI 10.1029/2007GL032276 PG 5 WC Geosciences, Multidisciplinary SC Geology GA 270IV UT WOS:000253715400002 ER PT J AU Deshler, T Mercer, JL Smit, HGJ Stubi, R Levrat, G Johnson, BJ Oltmans, SJ Kivi, R Thompson, AM Witte, J Davies, J Schmidlin, FJ Brothers, G Sasaki, T AF Deshler, Terry Mercer, Jennifer L. Smit, Herman G. J. Stubi, Rene Levrat, Gilbert Johnson, Bryan J. Oltmans, Samuel J. Kivi, Rigel Thompson, Anne M. Witte, Jacquelyn Davies, Jonathan Schmidlin, F. J. Brothers, G. Sasaki, Toru TI Atmospheric comparison of electrochemical cell ozonesondes from different manufacturers, and with different cathode solution strengths: The Balloon Experiment on Standards for Ozonesondes SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID GROUND-BASED LIDAR; INTERCOMPARISON CAMPAIGN; VERTICAL-DISTRIBUTION; OZONE PROFILES; STOIC 1989; TROPOSPHERIC OZONE; ECC; PHOTOMETER; ACCURACY; TRENDS AB A balloon flight to compare 18 ozonesondes with an ozone photometer and with ozone column measurements from Dobson and Brewer spectrophotometers was completed in April 2004. The core experiment consisted of 12 electrochemical concentration cell ozonesondes, 6 from Science Pump Corporation (SP) and 6 from ENSCI Corporation (ES), prepared with cathode solution concentrations of 0.5% KI (half buffer) and 1.0% KI (full buffer). Auxiliary ozonesondes consisted of two electrochemical concentration cell sondes with 2.0% KI (no buffer), two reconditioned sondes, and two Japanese-KC96 sondes. Precision of each group of similarly prepared ozonesondes was <2-3%. The six ozonesondes prepared according to the manufacturer's recommendations (SP, 1.0% KI, ES 0.5% KI) overestimated the photometer measurements by 5-10% in the stratosphere, but provided ozone columns in good agreement with the ground-based spectrophotometer measurements. This is consistent with the difference (similar to 5%) in ozone photometer and column measurements observed during the experiment. Using cathode cell concentrations of 1.0% KI for ES sondes caused overestimates of the photometer by 10-15% and of ozone column by 5-10%. In contrast, 0.5% KI in SP sondes led to good agreement with the photometer, but underestimates of ozone column. The KC96 sondes underestimated the photometer measurements by about 5-15% at air pressures above 30 hPa. Agreement was within 5% at lower pressures. Diluting the solution concentration and the buffers from 1.0% to 0.5% KI causes an approximately linear pressure-dependent decrease in ozone for both SP and ES sondes, ratio (0.5 KI/1.0 KI) = 0.9 + 0.024* log(10)(Pressure). C1 [Deshler, Terry; Mercer, Jennifer L.] Univ Wyoming, Dept Atmospher Sci, Laramie, WY 82071 USA. [Smit, Herman G. J.] Forschungszentrum Julich, Inst Chem & Dynam Geosphere 2, D-52425 Julich, Germany. [Stubi, Rene; Levrat, Gilbert] MeteoSwiss, Fed Off Meteorol & Climatol, Aerol Stn Payerne, CH-1530 Payerne, Switzerland. [Johnson, Bryan J.; Oltmans, Samuel J.] NOAA, Earth Syst Res Lab, Boulder, CO 80305 USA. [Kivi, Rigel] Finnish Meteorol Inst, Arctic Res Ctr, FIN-99600 Sodankyla, Finland. [Thompson, Anne M.] Penn State Univ, Dept Meteorol, University Pk, PA 16802 USA. [Witte, Jacquelyn] Sci Syst & Applicat Inc, Lanham, MD 20706 USA. [Schmidlin, F. J.; Brothers, G.] NASA, Goddard Space Flight Ctr, Wallops Flight Facil, Wallops Isl, VA 23337 USA. [Davies, Jonathan] Environm Canada, Air Qual Res Div, Toronto, ON M3H 5T4, Canada. [Witte, Jacquelyn] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Sasaki, Toru] Japan Meteorol Agcy, Tokyo, Japan. RP Deshler, T (reprint author), Univ Wyoming, Dept Atmospher Sci, Laramie, WY 82071 USA. EM deshler@uwyo.edu; mercer@uwyo.edu; h.smit@fz-juelich.de; rene.stubi@meteoswiss.ch; bryan.johnson@noaa.gov; samuel.j.oltmans@noaa.gov; rigel.kivi@fmi.fi; anne@met.psu.edu; witte@gavial.gsfc.nasa.gov; jonathan.davies@ec.gc.ca; fjs@osb1.wff.gsfc.gov; tsasaki@naps.kishou.go.jp RI Smit, Herman/J-2397-2012; Thompson, Anne /C-3649-2014 OI Smit, Herman/0000-0002-2268-4189; Thompson, Anne /0000-0002-7829-0920 NR 45 TC 58 Z9 60 U1 4 U2 7 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD FEB 29 PY 2008 VL 113 IS D4 AR D04307 DI 10.1029/2007JD008975 PG 17 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 270JA UT WOS:000253715900004 ER PT J AU Yang, YK Di Girolamo, L AF Yang, Yuekui Di Girolamo, Larry TI Impacts of 3-D radiative effects on satellite cloud detection and their consequences on cloud fraction and aerosol optical depth retrievals SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID CLEAR-SKY REFLECTANCE; SPATIAL-RESOLUTION; ALGORITHM; ISCCP; RADIANCES; MODIS; CLASSIFICATION; INSTRUMENTS; BRIGHTNESS; VALIDATION AB We present the first examination on how 3-D radiative transfer impacts satellite cloud detection that uses a single visible channel threshold. The 3-D radiative transfer through predefined heterogeneous cloud fields embedded in a range of horizontally homogeneous aerosol fields have been carried out to generate synthetic nadir-viewing satellite images at a wavelength of 0.67 mu m. The finest spatial resolution of the cloud field is 30 m. We show that 3-D radiative effects cause significant histogram overlap between the radiance distribution of clear and cloudy pixels, the degree to which depends on many factors (resolution, solar zenith angle, surface reflectance, aerosol optical depth (AOD), cloud top variability, etc.). This overlap precludes the existence of a threshold that can correctly separate all clear pixels from cloudy pixels. The region of clear/cloud radiance overlap includes moderately large (up to 5 in our simulations) cloud optical depths. Purpose-driven cloud masks, defined by different thresholds, are applied to the simulated images to examine their impact on retrieving cloud fraction and AOD. Large (up to 100s of %) systematic errors were observed that depended on the type of cloud mask and the factors that influence the clear/cloud radiance overlap, with a strong dependence on solar zenith angle. Different strategies in computing domain-averaged AOD were performed showing that the domain-averaged BRF from all clear pixels produced the smallest AOD biases with the weakest (but still large) dependence on solar zenith angle. The large dependence of the bias on solar zenith angle has serious implications for climate research that uses satellite cloud and aerosol products. C1 [Yang, Yuekui; Di Girolamo, Larry] Univ Illinois, Dept Atmospher Sci, Urbana, IL 61801 USA. RP Yang, YK (reprint author), Univ Maryland Baltimore Cty, Goddard Earth Sci & Technol Ctr, Baltimore, MD 21228 USA. EM yuekui@umbc.edu RI Yang, Yuekui/B-4326-2015 NR 49 TC 22 Z9 22 U1 0 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 FEB 29 PY 2008 VL 113 IS D4 AR D04213 DI 10.1029/2007JD009095 PG 20 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 270JA UT WOS:000253715900007 ER PT J AU Comiso, JC Steffen, K AF Comiso, Josefino C. Steffen, Konrad TI Introduction to special section on Large-Scale Characteristics of the Sea Ice Cover from AMSR-E and Other Satellite Sensors SO JOURNAL OF GEOPHYSICAL RESEARCH-OCEANS LA English DT Editorial Material C1 [Comiso, Josefino C.] NASA, Goddard Space Flight Ctr, Cryospher Sci Branch, Greenbelt, MD 20771 USA. [Steffen, Konrad] Univ Colorado, CIRES, Boulder, CO 80309 USA. RP Comiso, JC (reprint author), NASA, Goddard Space Flight Ctr, Cryospher Sci Branch, Greenbelt, MD 20771 USA. EM josefino.c.comiso@nasa.gov RI Steffen, Konrad/C-6027-2013 OI Steffen, Konrad/0000-0001-8658-1026 NR 27 TC 6 Z9 6 U1 0 U2 4 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9275 EI 2169-9291 J9 J GEOPHYS RES-OCEANS JI J. Geophys. Res.-Oceans PD FEB 29 PY 2008 VL 113 IS C2 AR C02S01 DI 10.1029/2007JC004442 PG 3 WC Oceanography SC Oceanography GA 270JH UT WOS:000253716600004 ER PT J AU Nieves-Chinchilla, T Vinas, AF AF Nieves-Chinchilla, Teresa Vinas, Adolfo F. TI Solar wind electron distribution functions inside magnetic clouds SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article ID CORONAL MASS EJECTIONS; KAPPA-DISTRIBUTIONS; AU; PARAMETERS; VOYAGER; PLASMAS; HELIOS; WAVES; CORE AB This paper presents a study of the kinetic properties of the electron velocity distribution functions within interplanetary magnetic clouds, since they are the dominant thermal component and can contribute as much as 50% of the total electron pressure within the clouds. The study is based on high time resolution data from the Goddard Space Flight Center Wind Solar Wind Experiment vector electron and ion spectrometer. Studies on interplanetary magnetic clouds have shown observational evidence of anticorrelation between the total electron density and temperature, which suggests a polytrope law P(e) = alpha n(e)(gamma) g for electrons with the constant gamma approximate to 0.5 < 1. This anticorrelation and small gamma values are interpreted in the context of the presence of highly non-Maxwellian electron distributions (i.e., nonthermal tails) within magnetic clouds. We have revisited some of the magnetic cloud events previously studied to quantify the nature of the nonthermal electrons by modeling the electron velocity distribution function using Maxwellian and kappa-like distribution functions to characterize the kinetic nonthermal effects. The results show that the electron density-temperature anticorrelation is not a unique feature of magnetic clouds. Within magnetic clouds, k values are generally small, in the range of 1.6-5.4; however, such small values are also typical of regions outside the clouds. We have shown that the density-temperature anticorrelation of the electron moments is persistently consistent with similar density-temperature anticorrelation in the electron halo component of the velocity distribution function and essentially little or no correlation was obtained for the core component. This result clearly shows that the temperature and density of the suprathermal components play a significant role in the temperature-density anticorrelation because of a relative enhancement of the halo component abundance to the total density. C1 [Nieves-Chinchilla, Teresa; Vinas, Adolfo F.] NASA, Goddard Space Flight Ctr, Geospace Phys Lab, Greenbelt, MD 20771 USA. RP Nieves-Chinchilla, T (reprint author), NASA, Goddard Space Flight Ctr, Geospace Phys Lab, Mail Code 673, Greenbelt, MD 20771 USA. EM adolfo.figueroa-vinas.1@gsfc.nasa.gov RI Nieves-Chinchilla, Teresa/F-3482-2016 OI Nieves-Chinchilla, Teresa/0000-0003-0565-4890 NR 32 TC 29 Z9 29 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 FEB 28 PY 2008 VL 113 IS A2 AR A02105 DI 10.1029/2007JA012703 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 270JV UT WOS:000253718000001 ER PT J AU Cockell, CS Mckay, CP Warren-Rhodes, K Horneck, G AF Cockell, Charles S. Mckay, Christopher P. Warren-Rhodes, Kim Horneck, Gerda TI Ultraviolet radiation-induced limitation to epilithic microbial growth in and deserts - Dosimetric experiments in the hyperarid core of the Atacama Desert SO JOURNAL OF PHOTOCHEMISTRY AND PHOTOBIOLOGY B-BIOLOGY LA English DT Article DE Atacama; desiccation; chroococcidiopsis; dosimetry; weathering ID UV-RADIATION; CHILE; MARS; LIFE; CHROOCOCCIDIOPSIS; MICROORGANISMS; CYANOBACTERIA; COMMUNITIES; ANTARCTICA; EXPOSURE AB Experiments were conducted during November 2003 in the dry core of the Atacama Desert, Yungay, Chile to test the hypothesis that UV radiation, in environments where liquid water is not available, and thus enzymatic repair of UV-induced damage is inhibited, can prevent epilithic colonization. Novel dosimeters made from the cryptoendolithic, desiccation and radiation-resistant cyanobacterium Chroococcidiopsis sp. isolated from the dry Negev desert, Israel, showed that monolayers of this organism were killed within one day. The diurnal profile of microbial loss of viability was investigated with dosimeters of Bacillus subtilis, which similarly showed cell death within one day. Soil grains obtained from south of Yungay where liquid water is more abundant and transported to the hyperarid core showed killing of indigenous vegetative organisms within one day. Gypsum and mineral grain coverings of I mm. were sufficient to prevent measurable UV-induced damage of Chroococcidiopsis and B. subtilis after 8 d exposure. These results show that under extreme desiccation and an ambient UV flux the surface of rocks can potentially be rendered sterile, but that millimetre thick mineral coverings can protect organisms from UV-induced killing, consistent with the observed patterns of lithophytic colonization in the Atacama Desert. These data further show that UV radiation can be an important limiting factor in surface biological rock weathering in and regions. (c) 2007 Elsevier B.V. All rights reserved. C1 [Cockell, Charles S.] Open Univ, PSSRI, Milton Keynes MK7 6AA, Bucks, England. [Mckay, Christopher P.; Warren-Rhodes, Kim] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Horneck, Gerda] DLR, Inst Aerospace Med, D-51170 Cologne, Germany. RP Cockell, CS (reprint author), Open Univ, PSSRI, Milton Keynes MK7 6AA, Bucks, England. EM c.s.cockell@open.ac.uk NR 33 TC 38 Z9 39 U1 1 U2 15 PU ELSEVIER SCIENCE SA PI LAUSANNE PA PO BOX 564, 1001 LAUSANNE, SWITZERLAND SN 1011-1344 J9 J PHOTOCH PHOTOBIO B JI J. Photochem. Photobiol. B-Biol. PD FEB 27 PY 2008 VL 90 IS 2 BP 79 EP 87 DI 10.1016/j.jphotobiol.2007.11.009 PG 9 WC Biochemistry & Molecular Biology; Biophysics SC Biochemistry & Molecular Biology; Biophysics GA 277MH UT WOS:000254216200001 PM 18191576 ER PT J AU Park, ES Ro, HW Nguyen, CV Jaffe, RL Yoon, DY AF Park, E. S. Ro, H. W. Nguyen, C. V. Jaffe, R. L. Yoon, D. Y. TI Infrared spectroscopy study of microstructures of poly(silsesquioxane)s SO CHEMISTRY OF MATERIALS LA English DT Article ID LOW-DIELECTRIC-CONSTANT; LOW-K DIELECTRICS; VIBRATIONAL STRUCTURE; STRUCTURAL CONTROL; THIN-FILMS; POLY(METHYLSILSESQUIOXANE)S; SILSESQUIOXANES; PRECURSORS AB Results are presented from theoretical and experimental infrared (IR) spectroscopy studies of the microstructures of poly(silsesquioxane)s (PSSQs) of varying chemical composition. The calculated IR spectra show two distinct asymmetric Si-O-Si stretch vibration bands for models of complete polyhedral cages, incomplete open cages, and short ladder structures. Close analyses of the calculated results indicate that the higher frequency IR band at about 1150 cm(-1) is derived from the parallel asymmetric Si-O-Si stretch vibration mode in the (Si-O)(n) ring subunit while the lower frequency band at about 1050 cm(-1) is due to the asymmetric Si-O-Si stretch symmetric with respect to the inversion point at the center of the (Si-O)(n) ring and is absent in highly symmetric cage structures. Experimentally, poly(methylsilses-quioxane) (PMSQ), poly(isobutylsilsesquioxane) (PiBSQ), and poly(phenylsilsesquioxane) (PPhSQ) exhibit a varying tendency of cage-like structures, rather than ladder structures, in as-polymerized samples. When the thermal conversion (curing) temperature is increased to 400 degrees C, the microstructure of PMSQ in thin solid films transforms from open cage-like structure toward a random network with lower symmetry. This change in microstructure is caused by the secondary condensation reaction and the evaporation of cage structures, and the effect of cage evaporation becomes most pronounced for PiBSQ films, which are mostly comprised of cage-like structures that evaporate around 280 degrees C. In comparison, PPhSQ films retain cage-like structure upon curing to 400 degrees C as a result of the high evaporation temperature (ca. 500 degrees C) of the cages. C1 [Park, E. S.; Ro, H. W.; Yoon, D. Y.] Seoul Natl Univ, Dept Chem, Seoul 151747, South Korea. [Nguyen, C. V.] ELORET, NASA, Ames Res Ctr, Moffett Field, CA 94305 USA. [Jaffe, R. L.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Yoon, DY (reprint author), Seoul Natl Univ, Dept Chem, Seoul 151747, South Korea. EM dyyoon@snu.ac.kr NR 33 TC 91 Z9 92 U1 4 U2 45 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 0897-4756 J9 CHEM MATER JI Chem. Mat. PD FEB 26 PY 2008 VL 20 IS 4 BP 1548 EP 1554 DI 10.1021/cm071575z PG 7 WC Chemistry, Physical; Materials Science, Multidisciplinary SC Chemistry; Materials Science GA 264JN UT WOS:000253283700059 ER PT J AU Kambe, E Ando, H Sato, B Izumiura, H Sekii, T Paulson, DB Yanagisawa, K Masuda, S Shibahashi, H Hatzes, AP Martic, M Lebrun, JC Mkrtichian, DE Kiss, LL Bruntt, H O'Toole, SJ Bedding, TR AF Kambe, Eiji Ando, Hiroyasu Sato, Bun'ei Izumiura, Hideyuki Sekii, Takashi Paulson, Diane B. Yanagisawa, Kenshi Masuda, Seiji Shibahashi, Hiromoto Hatzes, Artie P. Martic, Milena Lebrun, Jean-Claude Mkrtichian, David E. Kiss, Laszlo L. Bruntt, Hans O'Toole, Simon J. Bedding, Timothy R. TI Development of iodine cells for Subaru HDS and Okayama HIDES. III. An improvement on the radial-velocity measurement technique SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN LA English DT Article DE instrumentation : iodine cell; instrumentation : echelle spectrograph; stars : radial velocity; stars : planetary systems; stars : asteroseismology ID SOLAR-LIKE OSCILLATIONS; PLANET SEARCH PROGRAM; PROCYON-A; MODE FREQUENCIES; BETA-HYDRI; PRECISION; SPECTROGRAPH; CORE; MASS AB An improvement of the radial-velocity measurement accuracy is crucial for the detection of tiny stellar oscillations and exoplanets. Through the analysis of week-long extensive observations of solar-type stars (Procyon in 2000, 2002, and 2006/2007 and tau Cet in 2002 and 2006/2007), we have carefully examined, revised, and finely tuned the widely used multiple Gaussian IP fitting method for the spectrograph, HIDES. By determining a necessary and sufficient number of free parameters in the model as well as introducing an iterative process in the radial-velocity analysis, we can reach a precision of below 3 m s(-1), which is much smaller than the precision of 6 m s(-1) officially announced so far for HIDES. We also make our technique refined for the 2002 McDonald Procyon data. Even with our revised method, slow radial velocity variations with an amplitude of about 10 m s(-1) are left in the Procyon data. We emphasize that it is neither due to particular observing instruments nor radial-velocity analysis, and thus could be due to stellar origin. The analysis presented here makes the foundations of our next scientific analysis of the radial-velocity variations of Procyon, which will be presented in our forthcoming papers. C1 [Kambe, Eiji; Izumiura, Hideyuki; Yanagisawa, Kenshi] Natl Astron Observ Japan, Okayama Astrophys Observ, Asakuchi, Okayama 7190232, Japan. [Ando, Hiroyasu; Sekii, Takashi] Natl Astron Observ Japan, Mitaka, Tokyo 1818588, Japan. [Sato, Bun'ei] Tokyo Inst Technol, Meguro Ku, Tokyo 152, Japan. [Paulson, Diane B.] NASA, Goddard Space Flight Ctr, Planetary Syst Branch, Greenbelt, MD 20771 USA. [Masuda, Seiji] Tokushima Sci Museum, Astumn Land Tokushima, Tokushima 7790111, Japan. [Shibahashi, Hiromoto] Univ Tokyo, Sch Sci, Dept Astron, Bunkyo Ku, Tokyo 1130033, Japan. [Hatzes, Artie P.] Thuringer Landessternwarte, D-07778 Tautenburg, Germany. [Martic, Milena; Lebrun, Jean-Claude] CNRS, Serv Aeron, F-91371 Verrieres Le Buisson, France. [Mkrtichian, David E.] Sejong Univ, Astrophys Res Ctr Struct & Evolut Cosmos, Seoul 143747, South Korea. [Mkrtichian, David E.] Odessa Natl Univ, Astron Observ, UA-65014 Odessa, Ukraine. [Kiss, Laszlo L.; Bruntt, Hans; Bedding, Timothy R.] Univ Sydney, Sch Phys, Sydney, NSW 2006, Australia. [O'Toole, Simon J.] Anglo Australian Observ, Epping, NSW 1710, Australia. RP Kambe, E (reprint author), Natl Astron Observ Japan, Okayama Astrophys Observ, Asakuchi, Okayama 7190232, Japan. EM kambe@oao.nao.ac.jp RI Kiss, Laszlo/A-2539-2008; OI Bedding, Timothy/0000-0001-5943-1460; Bedding, Tim/0000-0001-5222-4661 NR 34 TC 8 Z9 8 U1 0 U2 2 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 FEB 25 PY 2008 VL 60 IS 1 BP 45 EP 53 DI 10.1093/pasj/60.1.45 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 300IR UT WOS:000255818000005 ER PT J AU Kahn, RA Chen, Y Nelson, DL Leung, FY Li, QB Diner, DJ Logan, JA AF Kahn, Ralph A. Chen, Yang Nelson, David L. Leung, Fok-Yan Li, Qinbin Diner, David J. Logan, Jennifer A. TI Wildfire smoke injection heights: Two perspectives from space SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID FOREST-FIRE SMOKE; TRANSPORT; PLUME AB The elevation at which wildfire smoke is injected into the atmosphere has a strong influence on how the smoke is dispersed, and is a key input to aerosol transport models. Aerosol layer height is derived with great precision from space-borne lidar, but horizontal sampling is very poor on a global basis. Aerosol height derived from space-borne stereo imaging is limited to source plumes having discernable features. But coverage is vastly greater, and captures the cores of major fires, where buoyancy can be sufficient to lift smoke above the near-surface boundary layer. Initial assessment of smoke injection from the Alaska-Yukon region during summer 2004 finds at least about 10% of wildfire smoke plumes reached the free troposphere. Modeling of smoke environmental impacts can benefit from the combined strengths of the stereo and lidar observations. C1 [Kahn, Ralph A.; Chen, Yang; Li, Qinbin; Diner, David J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Leung, Fok-Yan; Logan, Jennifer A.] Harvard Univ, Sch Engn & Appl Sci, Cambridge, MA 02138 USA. [Nelson, David L.] Columbus Technol & Serv Inc, Pasadena, CA 91101 USA. RP Kahn, RA (reprint author), NASA, Goddard Space Flight Ctr, Code 613-2, Greenbelt, MD 20771 USA. EM ralph.kahn@jpl.nasa.gov RI Chen, Yang/C-6529-2008; Kahn, Ralph/D-5371-2012 OI Chen, Yang/0000-0002-0993-7081; Kahn, Ralph/0000-0002-5234-6359 NR 13 TC 91 Z9 91 U1 2 U2 12 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD FEB 22 PY 2008 VL 35 IS 4 AR L04809 DI 10.1029/2007GL032165 PG 4 WC Geosciences, Multidisciplinary SC Geology GA 267TD UT WOS:000253531200002 ER PT J AU Sarantos, M Killen, RM Sharma, AS Slavin, JA AF Sarantos, Menelaos Killen, Rosemary M. Sharma, A. Surjalal Slavin, James A. TI Influence of plasma ions on source rates for the lunar exosphere during passage through the Earth's magnetosphere SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID STIMULATED DESORPTION; SODIUM ATOMS; MOON; SURFACE; ATMOSPHERES; MAGNETOTAIL; MODEL AB The total electron flux in the lunar exosphere, measured by the Electron Reflectometer onboard the Lunar Prospector during its passage through the Earth's magnetosphere (June 7-16, 1998), is strongly correlated with variations in the column abundance of equatorial sodium observed coincidentally with the McMath-Pierce solar telescope at Kitt Peak. At the same time, the exospheric temperature increased from a minimum of 1200 K to a maximum of 3000 K at minimum phase angle. A comparison of different source mechanisms, using the measured electron flux as the proxy for the ion flux, provides strong evidence that ion impact enhances the photon-stimulated desorption yield. At the Moon photon-stimulated desorption is shown to be the dominant source of exospheric sodium outside the magnetosphere. Inside the magnetosphere, where the ion flux and the associated photon-stimulated desorption yield decrease, the contributions from impact vaporization to the observed column abundance and temperature are found to be substantial. C1 [Sarantos, Menelaos; Killen, Rosemary M.; Sharma, A. Surjalal] Univ Maryland, Dept Astron, College Pk, MD 20771 USA. [Sarantos, Menelaos; Slavin, James A.] NASA, Goddard Space Flight Ctr, Heliophys Sci Div, Greenbelt, MD 20771 USA. RP Sarantos, M (reprint author), Univ Maryland, Dept Astron, College Pk, MD 20771 USA. EM sarantos@astro.umd.edu RI Slavin, James/H-3170-2012; Sarantos, Menelaos/H-8136-2013 OI Slavin, James/0000-0002-9206-724X; NR 13 TC 23 Z9 24 U1 1 U2 4 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 FEB 22 PY 2008 VL 35 IS 4 AR L04105 DI 10.1029/2007GL032310 PG 5 WC Geosciences, Multidisciplinary SC Geology GA 267TD UT WOS:000253531200003 ER PT J AU Monaghan, AJ Bromwich, DH Chapman, W Comiso, JC AF Monaghan, Andrew J. Bromwich, David H. Chapman, William Comiso, Josefino C. TI Recent variability and trends of Antarctic near-surface temperature SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID OCEAN SEA-ICE; HEMISPHERE ANNULAR MODE; POLAR MM5 SIMULATIONS; SOUTHERN-HEMISPHERE; CLIMATE VARIABILITY; MASS-BALANCE; OSCILLATION; CIRCULATION; REANALYSIS; ACCUMULATION AB A new monthly 1 degrees x 1 degrees Antarctic near-surface temperature reconstruction for 1960-2005 is presented. The use of numerical model fields to establish spatial relationships between fifteen continuous observational temperature records and the voids to which they are interpolated inherently accounts for the effects of the atmospheric circulation and topography on temperature variability. Employing a fixed observation network ensures that the reconstruction uncertainty remains constant in time. Comparison with independent observations indicates that the reconstruction and two other gridded observational temperature records are useful for evaluating regional near-surface temperature variability and trends throughout Antarctica. The reconstruction has especially good skill at reproducing temperature trends during the warmest months when melt contributes to ice sheet mass loss. The spatial variability of monthly near-surface temperature trends is strongly dependent on the season and time period analyzed. Statistically insignificant (p > 0.05) positive trends occur over most regions and months during 1960-2005. By contrast, 1970-2005 trends are weakly negative overall, consistent with positive trends in the Southern Hemisphere Annular Mode (SAM) during summer and autumn. Subtle near-surface temperature increases during winter from 1970 to 2000 are consistent with tropospheric warming from radiosonde records and a lack of winter SAM trends. Widespread but statistically insignificant (p > 0.05) warming over Antarctica from 1992 to 2005 coincides with a leveling off of upward SAM trends during summer and autumn since the mid-1990s. Weakly significant annual trends (p < 0.10) of about +1 K decade(-1) are found at three stations in interior and coastal East Antarctica since 1992. The subtle shift toward warming during the past 15 years raises the question of whether the recent trends are linked more closely to anthropogenic influences or multidecadal variability. C1 [Monaghan, Andrew J.; Bromwich, David H.] Ohio State Univ, Byrd Polar Res Ctr, Polar Meteorol Grp, Columbus, OH 43210 USA. [Bromwich, David H.] Ohio State Univ, Dept Geog, Atmospher Sci Program, Columbus, OH 43210 USA. [Chapman, William] Univ Illinois, Dept Atmospher Sci, Urbana, IL 61081 USA. [Comiso, Josefino C.] NASA, Goddard Space Flight Ctr, Cryospher Sci Branch, Greenbelt, MD 20771 USA. RP Monaghan, AJ (reprint author), Ohio State Univ, Byrd Polar Res Ctr, Polar Meteorol Grp, 1090 Carmack Rd, Columbus, OH 43210 USA. EM monaghan.11@osu.edu RI Bromwich, David/C-9225-2016; OI Monaghan, Andrew/0000-0002-8170-2359 NR 52 TC 66 Z9 68 U1 1 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 FEB 22 PY 2008 VL 113 IS D4 AR D04105 DI 10.1029/2007JD009094 PG 21 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 267TI UT WOS:000253531700006 ER PT J AU Comiso, JC Nishio, F AF Comiso, Josefino C. Nishio, Fumihiko TI Trends in the sea ice cover using enhanced and compatible AMSR-E, SSM/I, and SMMR data SO JOURNAL OF GEOPHYSICAL RESEARCH-OCEANS LA English DT Article ID PASSIVE MICROWAVE; SATELLITE; VARIABILITY; PARAMETERS; ALGORITHM; SURFACE AB Arguably, the most remarkable manifestation of change in the polar regions is the rapid decline in the Arctic perennial ice cover. Changes in the global sea ice cover, however, have been more modest, being only slightly negative in the Northern Hemisphere and even slightly positive in the Southern Hemisphere, the significance of which has not been adequately assessed because of unknown errors in the satellite historical data. Recent Advanced Microwave Scanning Radiometer (AMSR-E) high-resolution data are used as the baseline for generating an enhanced sea ice data set used in this study. Brightness temperature data from historical Special Scanning Microwave Imager (SSM/I) and Scanning Multichannel Microwave Radiometer (SMMR) sensors were normalized to be consistent with those from AMSR-E, and sea ice parameters were derived from all three data sets using the same algorithm for optimum consistency and accuracy. A small bias in sea ice extent is observed between AMSR- E and SSM/I data which, if uncorrected, causes an error of 0.62%/decade in the Arctic and 0.26%/decade in the Antarctic. Similar corrections are not needed in trend estimates of sea ice area. Biases due to seasonal changes in the accuracy of ice edge determinations, especially during melt periods, were also evaluated, and impacts on the trend results appear to be small. When updated to 2006, the trends in ice extent and area in the Arctic are now slightly more negative at -3.4 +/- 0.2 and -4.0 +/- 0.2% per decade, respectively, while the corresponding trends in the Antarctic remains slight but positive at 0.9 +/- 0.2 and 1.7 +/- 0.3% per decade. C1 [Comiso, Josefino C.] NASA, Goddard Space Flight Ctr, Cryospher Sci Branch, Greenbelt, MD USA. [Nishio, Fumihiko] Chiba Univ, Ctr Environm Remote Sensing, Chiba, Japan. RP Comiso, JC (reprint author), NASA, Goddard Space Flight Ctr, Cryospher Sci Branch, Greenbelt, MD USA. NR 30 TC 200 Z9 208 U1 12 U2 52 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 FEB 22 PY 2008 VL 113 IS C2 AR C02S07 DI 10.1029/2007JC004257 PG 22 WC Oceanography SC Oceanography GA 267TQ UT WOS:000253532500002 ER PT J AU Burlaga, LF Ness, NF Acuna, MH Wang, YM Sheeley, NR Wang, C Richardson, JD AF Burlaga, L. F. Ness, N. F. Acuna, M. H. Wang, Y. -M. Sheeley, N. R., Jr. Wang, C. Richardson, J. D. TI Global structure and dynamics of large-scale fluctuations in the solar wind: Voyager 2 observations during 2005 and 2006 SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article ID MERGED INTERACTION REGION; HELIOSPHERIC MAGNETIC-FIELD; OUTER HELIOSPHERE; PICKUP IONS; INTERPLANETARY SHOCKS; TERMINATION SHOCK; COSMIC-RAYS; 95 AU; SPEED; EVOLUTION AB The Voyager 2 (V2) observations of daily averages of the solar wind during 2005 and 2006 from 75.3 AU to 81.6 AU between approximate to 25.7 degrees S and 27.1 degrees S show both a step-like trend in the speed V(t) and "large-scale fluctuations'' of the magnetic field strength B, speed V, density N and temperature T. The distribution functions of B, N, and NV2 observed by V2 are lognormal and that of V is approximately Gaussian. We introduce a method for specifying the boundary conditions at all latitudes (except near the poles) on a Sun-centered surface of radius of 1 AU, based on solar magnetic field observations. This paper uses only the boundary conditions at the latitude of V2 and a 1-D time-dependent MHD model to calculate the radial evolution of the large-scale fluctuations of B(t), V(t) and N(t) at distances between 1 and 90 AU. This model explains the V2 observations of a lognormal distribution of B and the Gaussian distribution of V, but not the observed lognormal distributions of N and NV2. The lognormal distribution of B observed by V2 was produced primarily by dynamical processes beyond 1 AU. C1 [Burlaga, L. F.] NASA, Goddard Space Flight Ctr, Geospace Phys Lab, Greenbelt, MD 20771 USA. [Ness, N. F.] Catholic Univ Amer, Inst Astrophys & Computat Sci, Washington, DC 20064 USA. [Acuna, M. H.] NASA, Goddard Space Flight Ctr, Solar Syst Explorat Div, Greenbelt, MD 20771 USA. [Wang, Y. -M.; Sheeley, N. R., Jr.] USN, Res Lab, Washington, DC 20375 USA. [Wang, C.] Chinese Acad Sci, Ctr Space Sci & Appl Res, State Key Lab Space Weather, Beijing, Peoples R China. [Richardson, J. D.] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 37655 USA. RP Burlaga, LF (reprint author), NASA, Goddard Space Flight Ctr, Geospace Phys Lab, Code 673, Greenbelt, MD 20771 USA. EM leonard.f.burlaga@nasa.gov NR 55 TC 4 Z9 4 U1 0 U2 5 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9380 EI 2169-9402 J9 J GEOPHYS RES-SPACE JI J. Geophys. Res-Space Phys. PD FEB 22 PY 2008 VL 113 IS A2 AR A02104 DI 10.1029/2007JA012796 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 267UK UT WOS:000253534500005 ER PT J AU Forbes, JM Zhang, X Palo, S Russell, J Mertens, CJ Mlynczak, M AF Forbes, J. M. Zhang, X. Palo, S. Russell, J. Mertens, C. J. Mlynczak, M. TI Tidal variability in the ionospheric dynamo region SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article ID NONMIGRATING DIURNAL TIDES; GENERAL-CIRCULATION MODEL; LATENT-HEAT RELEASE; UPPER-ATMOSPHERE; SEMIDIURNAL TIDES; MIDDLE ATMOSPHERE; THERMOSPHERE; TEMPERATURE; WINDS; UARS AB The seasonal and interannual variability of migrating (Sun-synchronous) and nonmigrating solar atmospheric tides at altitudes between 100 and 116 km are investigated using temperature measurements made with the SABER instrument on the TIMED spacecraft during 2002-2006. Quasi-biennial variations of order +/- 10-15% in migrating diurnal and semidiurnal tidal amplitudes are found, presumably due to modulation by the quasi-biennial oscillation (QBO) as the tides propagate from their troposphere and stratospheric sources to the lower thermosphere. A number of nonmigrating tidal components are found that have the potential to produce significant longitudinal variability of the total tidal fields. The most prominent of these, i.e., those that appear at amplitudes of order 5-10 K in a 5-year mean climatology, include the zonally symmetric (s = 0) diurnal tide (D0); the eastward propagating diurnal and semidiurnal tides with zonal wave numbers s = -2 (DE2 and SE2) and s = -3 (DE3 and SE3); and the following westward propagating waves: diurnal s = 2 (DW2); semidiurnal s = 1 (SW1), s = 3 (SW3), and s = 4 (SW4); and terdiurnal s = 5 (TW5). These waves can be plausibly accounted for by nonlinear interaction between migrating tidal components and stationary planetary waves with s = 1 or s = 2 or by longitudinal variations of tropospheric thermal forcing. Additional waves that occur during some years or undergo phase cancellation within construction of a 5-year climatology include DW5, SE1, SE4, SW6, TE1, TW1, and TW7. It is anticipated that the winds that accompany all of these waves in the 100-170 km region will impose longitudinal variability in the electric fields produced through the ionospheric dynamo mechanism, thereby modulating vertical motion of the equatorial ionosphere and the concomitant plasma densities. In addition to the wave-4 modulation of the equatorial ionosphere that has recently been discovered and replicated in modeling studies, the waves revealed here will generate wave-1 (SW1, SW3, D0, DW2), wave-2 (SW4, TW1), wave-3 (DE2, SE1), wave-4 (DE3, SE2, DW5, SW6, TE1, TW7), wave-5 (SE3), and wave-6 (SE4) components of this ionospheric variability, depending on year and time of year. However, the absolute and relative efficiencies with which these waves produce electric fields remains to be determined. C1 [Forbes, J. M.; Zhang, X.; Palo, S.] Univ Colorado, Dept Aerosp Engn Sci, Boulder, CO 80309 USA. [Russell, J.] Hampton Univ, Ctr Atmospher Sci, Hampton, VA 23668 USA. [Mertens, C. J.; Mlynczak, M.] NASA, Langley Res Ctr, Hampton, VA 23681 USA. RP Forbes, JM (reprint author), Univ Colorado, Dept Aerosp Engn Sci, UCB 429, Boulder, CO 80309 USA. EM forbes@colorado.edu RI Mlynczak, Martin/K-3396-2012; OI FORBES, JEFFREY/0000-0001-6937-0796; PALO, SCOTT/0000-0002-4729-4929 NR 39 TC 159 Z9 159 U1 3 U2 15 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 FEB 22 PY 2008 VL 113 IS A2 AR A02310 DI 10.1029/2007JA012737 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 267UK UT WOS:000253534500004 ER PT J AU Syed, TH Famiglietti, JS Rodell, M Chen, J Wilson, CR AF Syed, Tajdarul H. Famiglietti, James S. Rodell, Matthew Chen, Jianli Wilson, Clark R. TI Analysis of terrestrial water storage changes from GRACE and GLDAS SO WATER RESOURCES RESEARCH LA English DT Article ID CLIMATE EXPERIMENT GRACE; TIME-VARIABLE GRAVITY; SOIL-MOISTURE; MASS-LOSS; RECOVERY; FIELD; EVAPOTRANSPIRATION; VARIABILITY; ILLINOIS; SYSTEM AB [1] Since March 2002, the Gravity Recovery and Climate Experiment (GRACE) has provided first estimates of land water storage variations by monitoring the time-variable component of Earth's gravity field. Here we characterize spatial-temporal variations in terrestrial water storage changes (TWSC) from GRACE and compare them to those simulated with the Global Land Data Assimilation System (GLDAS). Additionally, we use GLDAS simulations to infer how TWSC is partitioned into snow, canopy water and soil water components, and to understand how variations in the hydrologic fluxes act to enhance or dissipate the stores. Results quantify the range of GRACE-derived storage changes during the studied period and place them in the context of seasonal variations in global climate and hydrologic extremes including drought and flood, by impacting land memory processes. The role of the largest continental river basins as major locations for freshwater redistribution is highlighted. GRACE-based storage changes are in good agreement with those obtained from GLDAS simulations. Analysis of GLDAS-simulated TWSC illustrates several key characteristics of spatial and temporal land water storage variations. Global averages of TWSC were partitioned nearly equally between soil moisture and snow water equivalent, while zonal averages of TWSC revealed the importance of soil moisture storage at low latitudes and snow storage at high latitudes. Evapotranspiration plays a key role in dissipating globally averaged terrestrial water storage. Latitudinal averages showed how precipitation dominates TWSC variations in the tropics, evapotranspiration is most effective in the midlatitudes, and snowmelt runoff is a key dissipating flux at high latitudes. Results have implications for monitoring water storage response to climate variability and change, and for constraining land model hydrology simulations. C1 [Syed, Tajdarul H.; Famiglietti, James S.] Univ Calif Irvine, Dept Earth Syst Sci, Irvine, CA 92717 USA. [Rodell, Matthew] NASA, Goddard Space Flight Ctr, Hydrol Sci Branch, Greenbelt, MD 20771 USA. [Chen, Jianli] Univ Texas Austin, Ctr Space Res, Austin, TX 78712 USA. [Wilson, Clark R.] Univ Texas Austin, Dept Geol Sci, Austin, TX 78712 USA. RP Syed, TH (reprint author), Univ Calif Irvine, Dept Earth Syst Sci, Irvine, CA 92717 USA. RI Rodell, Matthew/E-4946-2012; Syed, Tajdarul/G-6731-2014 OI Rodell, Matthew/0000-0003-0106-7437; NR 48 TC 145 Z9 155 U1 9 U2 72 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0043-1397 EI 1944-7973 J9 WATER RESOUR RES JI Water Resour. Res. PD FEB 22 PY 2008 VL 44 IS 2 AR W02433 DI 10.1029/2006WR005779 PG 15 WC Environmental Sciences; Limnology; Water Resources SC Environmental Sciences & Ecology; Marine & Freshwater Biology; Water Resources GA 267VA UT WOS:000253536100001 ER PT J AU Schafer, JS Eck, TF Holben, BN Artaxo, P Duarte, AF AF Schafer, J. S. Eck, T. F. Holben, B. N. Artaxo, P. Duarte, A. F. TI Characterization of the optical properties of atmospheric aerosols in Amazonia from long-term AERONET monitoring (1993-1995 and 1999-2006) SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID SKY RADIANCE MEASUREMENTS; BIOMASS BURNING AEROSOLS; SINGLE SCATTERING ALBEDO; SAHARAN DUST; BRAZIL; BASIN; DEPTH; WATER; SUN; VARIABILITY AB We present a new climatology of atmospheric aerosols (primarily pyrogenic and biogenic) for the Brazilian tropics on the basis of a high-quality data set of spectral aerosol optical depth and directional sky radiance measurements from Aerosol Robotic Network (AERONET) Cimel Sun-sky radiometers at more than 15 sites distributed across the Amazon basin and adjacent Cerrado region. This network is the only long-term project (with a record including observations from more than 11 years at some locations) ever to have provided ground-based remotely-sensed column aerosol properties for this critical region. Distinctive features of the Amazonian area aerosol are presented by partitioning the region into three aerosol regimes: southern Amazonian forest, Cerrado, and northern Amazonian forest. The monitoring sites generally include measurements from the interval 1999-2006, but some sites have measurement records that date back to the initial days of the AERONET program in 1993. Seasonal time series of aerosol optical depth (AOD), angstrom ngstrom exponent, and columnar-averaged microphysical properties of the aerosol derived from sky radiance inversion techniques (single-scattering albedo, volume size distribution, fine mode fraction of AOD, etc.) are described and contrasted for the defined regions. During the wet season, occurrences of mineral dust penetrating deep into the interior were observed. C1 [Schafer, J. S.] Sci Syst & Applicat Inc, Lanham, MD 20706 USA. [Schafer, J. S.; Eck, T. F.; Holben, B. N.] NASA, Goddard Space Flight Ctr, Biospher Sci Branch, Greenbelt, MD 20771 USA. [Eck, T. F.] Univ Maryland Baltimore Cty, Goddard Earth Sci & Technol Ctr, Baltimore, MD 21228 USA. [Artaxo, P.] Univ Sao Paulo, Inst Fis, Dept Fis Aplicada, BR-05508900 Sao Paulo, Brazil. [Duarte, A. F.] Univ Fed Acre, Dept Ciencias Nat, BR-69915900 Rio Branco, AC, Brazil. RP Schafer, JS (reprint author), Sci Syst & Applicat Inc, 10210 Greenbelt Rd,Suite 600, Lanham, MD 20706 USA. EM joel.schafer@nasa.gov RI Schafer, Joel/A-3978-2010; ECK, THOMAS/D-7407-2012; Artaxo, Paulo/E-8874-2010 OI Artaxo, Paulo/0000-0001-7754-3036 NR 40 TC 40 Z9 40 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 FEB 21 PY 2008 VL 113 IS D4 AR D04204 DI 10.1029/2007JD009319 PG 16 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 267TH UT WOS:000253531600002 ER PT J AU Comiso, JC Parkinson, CL AF Comiso, Josefino C. Parkinson, Claire L. TI Arctic sea ice parameters from AMSR-E data using two techniques and comparisons with sea ice from SSM/I SO JOURNAL OF GEOPHYSICAL RESEARCH-OCEANS LA English DT Article ID PASSIVE MICROWAVE; ALGORITHM; COVER; SMMR; GHZ AB We use two algorithms to process Advanced Microwave Scanning Radiometer for the Earth Observing System (AMSR-E) data in order to determine algorithm dependence, if any, on the estimates of sea ice concentration, ice extent and area, and trends and to evaluate how AMSR-E data compare with historical Special Sensor Microwave Imager (SSM/I) data. The monthly ice concentrations derived from the two algorithms from AMSR-E data (the AMSR-E bootstrap algorithm, or ABA, and the enhanced NASA team algorithm, or NT2), differ on average by about 1-3%, with data from the consolidated ice region being comparable for ABA and NT2 retrievals while data in the marginal ice zones and thin ice regions show slightly higher values when the NT2 algorithm is used. The ice extents and areas derived separately from AMSR-E using these two algorithms are, however, in good agreement, with the differences (ABA - NT2) being about 0.07 x 10(6) km(2) on average for ice extents and -0.07 x 10(6) km(2) for ice area, which are small compared with mean seasonal values of 10.5 x 10(6) and 9.8 x 10(6) for ice extent and area, respectively. Likewise, extents and areas derived from the same algorithm but from AMSR-E and SSM/I data are consistent but differ by about 0.24 x 10(6) km(2) and 0.14 x 10(6) km(2), respectively. The discrepancies are larger with the estimates of extents than area mainly because of differences in channel selection and sensor resolutions. Trends in extent during the AMSR-E era were also estimated, and results from all three data sets are shown to be in good agreement (within errors). C1 [Comiso, Josefino C.; Parkinson, Claire L.] NASA, Goddard Space Flight Ctr, Cryospher Sci Branch, Greenbelt, MD 20771 USA. RP Comiso, JC (reprint author), NASA, Goddard Space Flight Ctr, Cryospher Sci Branch, Code 614-1, Greenbelt, MD 20771 USA. EM josefino.c.comiso@nasa.gov RI Parkinson, Claire/E-1747-2012 OI Parkinson, Claire/0000-0001-6730-4197 NR 28 TC 18 Z9 20 U1 2 U2 9 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 FEB 21 PY 2008 VL 113 IS C2 AR C02S05 DI 10.1029/2007JC004255 PG 16 WC Oceanography SC Oceanography GA 267TP UT WOS:000253532400001 ER PT J AU Starling, RLC O'Brien, PT Willingale, R Page, KL Osborne, JP De Pasquale, M Nakagawa, YE Kuin, NPM Onda, K Norris, JP Ukwatta, TN Kodaka, N Burrows, DN Kennea, JA Page, MJ Perri, M Markwardt, CB AF Starling, R. L. C. O'Brien, P. T. Willingale, R. Page, K. L. Osborne, J. P. De Pasquale, M. Nakagawa, Y. E. Kuin, N. P. M. Onda, K. Norris, J. P. Ukwatta, T. N. Kodaka, N. Burrows, D. N. Kennea, J. A. Page, M. J. Perri, M. Markwardt, C. B. TI Swift captures the spectrally evolving prompt emission of GRB070616 SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE gamma-rays : bursts ID GAMMA-RAY-BURSTS; AFTERGLOW EMISSION; HOST-GALAXY; LONG; RADIATION; BATSE; TELESCOPE; MODELS; DUST; GRBS AB The origins of gamma-ray burst (GRB) prompt emission are currently not well understood and in this context long, well-observed events are particularly important to study. We present the case of GRB 070616, analysing the exceptionally long-duration multipeaked prompt emission, and later afterglow, captured by all the instruments on-board Swift and by Suzaku Wide-Band All-Sky Monitor (WAM). The high-energy light curve remained generally flat for several hundred seconds before going into a steep decline. Spectral evolution from hard to soft is clearly taking place throughout the prompt emission, beginning at 285 s after the trigger and extending to 1200 s. We track the movement of the spectral peak energy, whilst observing a softening of the low-energy spectral slope. The steep decline in flux may be caused by a combination of this strong spectral evolution and the curvature effect. We investigate origins for the spectral evolution, ruling out a superposition of two power laws and considering instead an additional component dominant during the late prompt emission. We also discuss origins for the early optical emission and the physics of the afterglow. The case of GRB 070616 clearly demonstrates that both broad-band coverage and good time resolution are crucial to pin down the origins of the complex prompt emission in GRBs. C1 [Starling, R. L. C.; O'Brien, P. T.; Willingale, R.; Page, K. L.; Osborne, J. P.] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England. [De Pasquale, M.; Kuin, N. P. M.; Page, M. J.] UCL, Mullard Space Sci Lab, Dorking RH5 6NT, Surrey, England. [Nakagawa, Y. E.] Aoyama Gakuin Univ, Dept Phys & Math, Sagamihara, Kanagawa 2298558, Japan. [Onda, K.; Kodaka, N.] Saitama Univ, Dept Phys, Saitama 3388570, Japan. [Norris, J. P.] Univ Denver, Denver Res Inst, Denver, CO 80208 USA. [Norris, J. P.] Stanford Univ, Stanford, CA 94305 USA. [Ukwatta, T. N.; Markwardt, C. B.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Ukwatta, T. N.] George Washington Univ, Dept Phys, Ctr Nucl Studies, Washington, DC 20052 USA. [Burrows, D. N.; Kennea, J. A.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Perri, M.] ASI Sci Data Ctr, I-00044 Frascati, Italy. [Markwardt, C. B.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. RP Starling, RLC (reprint author), Univ Leicester, Dept Phys & Astron, Univ Rd, Leicester LE1 7RH, Leics, England. EM rlcs1@star.le.ac.uk RI XRAY, SUZAKU/A-1808-2009; OI Perri, Matteo/0000-0003-3613-4409 NR 64 TC 19 Z9 20 U1 1 U2 3 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD FEB 21 PY 2008 VL 384 IS 2 BP 504 EP 514 DI 10.1111/j.1365-2966.2007.12763.x PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 259HS UT WOS:000252931000006 ER PT J AU Raymond, SN Barnes, R Mandell, AM AF Raymond, Sean N. Barnes, Rory Mandell, Avi M. TI Observable consequences of planet formation models in systems with close-in terrestrial planets SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Review DE astrobiology; methods : N-body simulations; methods : numerical; planetary systems : formation; planetary systems : protoplanetary discs ID EARTH-LIKE PLANETS; EXTRASOLAR GIANT PLANETS; LOW-MASS STARS; MAIN-SEQUENCE STARS; T-TAURI STARS; M-CIRCLE-PLUS; M-DWARF STARS; SOLAR NEBULA; SUPER-EARTHS; PROTOPLANETARY DISKS AB To date, two planetary systems have been discovered with close-in, terrestrial-mass planets (less than or similar to 5 -10M(circle plus)). Many more such discoveries are anticipated in the coming years with radial velocity and transit searches. Here we investigate the different mechanisms that could form 'hot Earths' and their observable predictions. Models include: (1) in situ accretion; (2) formation at larger orbital distance followed by inward 'type 1' migration; (3) formation from material being 'shepherded' inward by a migrating gas giant planet; (4) formation from material being shepherded by moving secular resonances during dispersal of the protoplanetary disc; (5) tidal circularization of eccentric terrestrial planets with close-in perihelion distances and (6) photoevaporative mass-loss of a close-in giant planet. Models 1-4 have been validated in previous work. We show that tidal circularization can form hot Earths, but only for relatively massive planets (greater than or similar to 5M(circle plus)) with very close-in perihelion distances (less than or similar to 0.025 au), and even then the net inward movement in orbital distance is at most only 0.1-0.15 au. For planets of less than similar to 70M(circle plus), photoevaporation can remove the planet's envelope and leave behind the solid core on a Gyr time-scale, but only for planets inside 0.025-0.05 au. Using two quantities that are observable by current and upcoming missions, we show that these models each produce unique signatures, and can be observationally distinguished. These observables are the planetary system architecture (detectable with radial velocities, transits and transit timing) and the bulk composition of transiting close-in terrestrial planets (measured by transits via the planet's radius). C1 [Raymond, Sean N.] Univ Colorado, Ctr Astrophys & Space Astron, Boulder, CO 80309 USA. [Barnes, Rory] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA. [Mandell, Avi M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Raymond, SN (reprint author), Univ Colorado, Ctr Astrophys & Space Astron, Boulder, CO 80309 USA. EM raymond@lasp.colorado.edu RI Mandell, Avi/F-9361-2012 NR 165 TC 71 Z9 71 U1 1 U2 3 PU BLACKWELL PUBLISHING PI OXFORD PA 9600 GARSINGTON RD, OXFORD OX4 2DQ, OXON, ENGLAND SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD FEB 21 PY 2008 VL 384 IS 2 BP 663 EP 674 DI 10.1111/j.1365-2966.2007.12712.x PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 259HS UT WOS:000252931000019 ER PT J AU McGowan, KE Coe, MJ Schurch, MPE Corbet, RHD Galache, JL Udalski, A AF McGowan, K. E. Coe, M. J. Schurch, M. P. E. Corbet, R. H. D. Galache, J. L. Udalski, A. TI Optical and X-ray variability of two Small Magellanic Cloud X-ray binary pulsars - SXP46.6 and SXP6.85 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; MACHO PHOTOMETRY; OUTBURSTS; ACCRETION; BEHAVIOR; PERIOD; STARS; SMC AB We present long-term optical and RXTE data of two X-ray binary pulsars in the Small Magellanic Cloud, SXP46.6 and SXP6.85. The optical light curves of both sources show substantial (similar to 0.5-0.8 mag) changes over the time-span of the observations. While the optical data for SXP6.85 do not reveal any periodic behaviour, by detrending the optical measurements for SXP46.6 we find an orbital period of similar to 137 d, consistent with results from the X-ray data. The detection of Type I X-ray outbursts from SXP46.6, combined with the fact that we also see optical outbursts at these times, implies that SXP46.6 is a high orbital eccentricity system. Using contemporaneous optical spectra of SXP46.6, we find that the equivalent width of the H alpha emission line changes over time indicating that the size of the circumstellar disc varies. By studying the history of the colour variations for SXP6.85, we find that the source gets redder as it brightens which can also be attributed to changes in the circumstellar disc. We do not find any correlation between the X-ray and optical data for SXP6.85. The results for SXP6.85 suggest that it is a low-eccentricity binary and that the optical modulations are due to the Be phenomenon. C1 [McGowan, K. E.; Coe, M. J.; Schurch, M. P. E.] Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England. [Corbet, R. H. D.] Univ Maryland, NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Galache, J. L.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Udalski, A.] Warsaw Univ Obsev, PL-00478 Warsaw, Poland. RP McGowan, KE (reprint author), Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England. EM kem@astro.soton.ac.uk NR 29 TC 18 Z9 18 U1 0 U2 0 PU BLACKWELL PUBLISHING PI OXFORD PA 9600 GARSINGTON RD, OXFORD OX4 2DQ, OXON, ENGLAND SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD FEB 21 PY 2008 VL 384 IS 2 BP 821 EP 826 DI 10.1111/j.1365-2966.2007.12762.x PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 259HS UT WOS:000252931000034 ER PT J AU Saif, B Bluth, M Greenfield, P Hack, W Eegholm, BH Blake, P Keski-Kuha, R Feinberg, L Arenberg, JW AF Saif, Babak Bluth, Marcel Greenfield, Perry Hack, Warren Eegholm, Bente Hoffmann Blake, Peter Keski-Kuha, Ritva Feinberg, Lee Arenberg, Jonathan W. TI Measurement of large cryogenic structures using a spatially phase-shifted digital speckle pattern interferometer SO APPLIED OPTICS LA English DT Article AB The James Webb Space Telescope (JWST) Backplane Stability Test Article (BSTA) was developed to demonstrate large precision cryogenic structures' technology readiness for use in the JWST The thermal stability of the BSTA was measured at cryogenic temperatures at the Marshall Space Flight Center (MSFC) X-Ray Calibration Facility (XRCF) and included nearly continuous measurements over a six-week period in the summer of 2006 covering the temperature range from ambient down to 30 Kusing a spatially phase-shifted digital speckle pattern interferometer (SPS-DSPI). The BSTA is a full size, one-sixth section of the JWST primary mirror backplane assembly (PMBA). The BSTA, measuring almost 3 m across, contains most of the prominent structural elements of the backplane and is to our knowledge the largest structure ever measured with SPS-DSPI at cryogenic conditions. The SPS-DSPI measured rigid body motion and deformations of BSTA to nanometer-level accuracy. The SPS-DSPI was developed specifically for the purposes of this test and other tests of large cryogenic structures for JWST. (c) 2008 Optical Society of America. C1 [Saif, Babak; Greenfield, Perry; Hack, Warren; Eegholm, Bente Hoffmann] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Bluth, Marcel] Alliant Tech Syst, Space Syst Grp, Magna, UT 84044 USA. [Blake, Peter; Keski-Kuha, Ritva; Feinberg, Lee] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Arenberg, Jonathan W.] Northrop Grumman Space Technol, Redondo Beach, CA 90278 USA. RP Eegholm, BH (reprint author), Space Telescope Sci Inst, 3700 San Martin Dr, Baltimore, MD 21218 USA. EM beegholm@stsci.edu OI Arenberg, Jonathan/0000-0003-1096-5634 NR 10 TC 10 Z9 10 U1 0 U2 2 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 FEB 20 PY 2008 VL 47 IS 6 BP 737 EP 745 DI 10.1364/AO.47.000737 PG 9 WC Optics SC Optics GA 276LA UT WOS:000254141800003 PM 18288221 ER PT J AU Winter, LM Mushotzky, RF Tueller, J Markwardt, C AF Winter, Lisa M. Mushotzky, Richard F. Tueller, Jack Markwardt, Craig TI X-ray properties of an unbiased hard X-ray-detected sample of active galactic nuclei SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : active; surveys; X-rays : galaxies ID XMM-NEWTON OBSERVATIONS; SEYFERT 1 GALAXIES; K-ALPHA LINE; ASCA OBSERVATIONS; TIME VARIABILITY; COMPTON-THICK; OPTICAL SPECTROSCOPY; HOST GALAXIES; BRIGHTEST AGN; LOCKMAN HOLE AB The Swift gamma-ray observatory's Burst Alert Telescope (BAT) has detected a sample of AGNs based solely on their hard X-ray flux (14-195 keV). In this paper we present for the first time XMM-Newton X-ray spectra for 22 BAT AGNs with no previously analyzed X-ray spectra. If our sources are a representative sample of the BAT AGNs, as we claim, our results present for the first time global X-ray properties of an unbiased toward absorption (n(H) < 3 x 10(25) cm(-2)), local (< z > = 0.03), AGN sample. We find 9/22 low-absorption (n(H) < 10(23) cm(-2)), simple power-law model sources, where 4 of these sources have a statistically significant soft component. Among these sources, we find the presence of a warm absorber statistically significant for only one Seyfert 1 source, contrasting with the ASCA results of Reynolds and George and coworkers, who find signatures of warm absorption in half or more of their Seyfert 1 samples at similar redshifts. In addition, the remaining sources (13/22) have more complex spectra, well fitted by an absorbed power law at E > 2.0 keV. Five of the complex sources are classified as Compton-thick candidates. Further, we find four more sources with properties consistent with the hidden/buried AGNs reported by Ueda and coworkers. Finally, we include a comparison of the XMM-Newton EPIC spectra with available Swift X-Ray Telescope (XRT) observations. From these comparisons, we find 6/16 sources with varying column densities, 6/16 sources with varying power-law indices, and 13/16 sources with varying fluxes, over periods of hours to months. Flux and power-law index are correlated for objects where both parameters vary. C1 [Winter, Lisa M.; Markwardt, Craig] Univ Maryland, College Pk, MD 20742 USA. [Mushotzky, Richard F.; Tueller, Jack; Markwardt, Craig] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Winter, LM (reprint author), Univ Maryland, College Pk, MD 20742 USA. EM lwinter@astro.umd.edu RI Tueller, Jack/D-5334-2012; OI Winter, Lisa/0000-0002-3983-020X NR 38 TC 70 Z9 71 U1 0 U2 0 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 FEB 20 PY 2008 VL 674 IS 2 BP 686 EP 710 DI 10.1086/525274 PG 25 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 266RK UT WOS:000253454500008 ER PT J AU Franklin, J Snell, RL Kaufman, MJ Melnick, GJ Neufeld, DA Hollenbach, DJ Bergin, EA AF Franklin, Jonathan Snell, Ronald L. Kaufman, Michael J. Melnick, Gary J. Neufeld, David A. Hollenbach, David J. Bergin, Edwin A. TI SWAS observations of water in molecular outflows SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM : abundances; ISM : jets and outflows; ISM : molecules; stars : formation; stars : winds; outflows ID WAVE-ASTRONOMY-SATELLITE; SERPENS CLOUD CORE; ORION-KL; C-I; VAPOR EMISSION; STAR-FORMATION; LINE SURVEY; HH 24-26; GAS; H2O AB We present detections of the ground-state 1(10) -> 1(01) transition of ortho-H2O at 557 GHz in 18 molecular outflows based on data from the Submillimeter Wave Astronomy Satellite (SWAS). These results are combined with ground-based observations of the J = 1-0 transitions of (CO)-C-12 and (CO)-C-13 obtained at the Five College Radio Astronomy Observatory (FCRAO). Data from Infrared Space Observatory (ISO) for a subset of the outflows are also discussed. Assuming that the SWAS water-line emission originates from the same gas traced by CO emission, we find that the outflowing gas in most outflows has an ortho-H2O abundance relative to H-2 of between similar to 10(-7) and 10(-6). Analysis of the water abundance as a function of outflow velocity reveals a strong dependence. The abundance of ortho-H2O increases with velocity, and at the highest outflow velocities some of the outflows have relative ortho-H2O abundances of order 10(-4). However, the mass of very high velocity gas with such elevated H2O abundances represents less than 1% of the total outflow gas mass. The ISO LWS observations of high-J rotational lines of CO and the 179.5 mu m transition of ortho-H2O provide evidence for a warmer outflow component than required to produce either the SWAS or FCRAO lines. The ISO line-flux ratios can be reproduced with C-shock models with shock velocities of order 25 km s(-1) and pre-shock densities of order 10(5) cm(-3); these C-shocks have postshock relative water abundances greater than 10(-4). The mass associated with the ISO emission is also quite small compared with the total outflow mass and is similar to that responsible for the highest velocity water emission detected by SWAS. Although the gas responsible for the ISO emission has elevated levels of water, the bulk of the outflowing gas has an abundance of ortho-H2O well below what would be expected if the gas has passed through a C-shock with shock velocities greater than 10 km s(-1). Gas-phase water can be depleted in the postshock gas due to freezeout onto grain mantles; however, the rate of freezeout is too slow to explain our results. Therefore, we believe that only a small fraction of the outflowing molecular gas has passed through shocks strong enough to fully convert the gas-phase oxygen to water. This result has implications for the acceleration mechanism of the molecular gas in these outflows. C1 [Franklin, Jonathan; Snell, Ronald L.] Univ Massachusetts, Dept Astron, Amherst, MA 01003 USA. [Kaufman, Michael J.] San Jose State Univ, Dept Phys, San Jose, CA 95192 USA. [Melnick, Gary J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Neufeld, David A.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Hollenbach, David J.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Bergin, Edwin A.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. RP Franklin, J (reprint author), Univ Massachusetts, Dept Astron, LGRT 619,710 N Pleasant St, Amherst, MA 01003 USA. NR 54 TC 38 Z9 38 U1 0 U2 1 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 FEB 20 PY 2008 VL 674 IS 2 BP 1015 EP 1031 DI 10.1086/524924 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 266RK UT WOS:000253454500028 ER PT J AU Trilling, DE Bryden, G Beichman, CA Rieke, GH Su, KYL Stansberry, JA Blaylock, M Stapelfeldt, KR Beeman, JW Haller, EE AF Trilling, D. E. Bryden, G. Beichman, C. A. Rieke, G. H. Su, K. Y. L. Stansberry, J. A. Blaylock, M. Stapelfeldt, K. R. Beeman, J. W. Haller, E. E. TI Debris disks around Sun-like stars SO ASTROPHYSICAL JOURNAL LA English DT Article DE circumstellar matter; infrared : stars; planetary systems : formation ID SOLAR-TYPE STARS; MAIN-SEQUENCE STARS; MULTIBAND IMAGING PHOTOMETER; SPITZER MIPS SURVEY; BOLOMETRIC CORRECTIONS; INFRARED PHOTOMETRY; PLANETARY SYSTEM; DWARF STARS; FGK STARS; F-DWARF AB We have observed nearly 200 FGK stars at 24 and 70 mu m with the Spitzer Space Telescope. We identify excess infrared emission, including a number of cases where the observed flux is more than 10 times brighter than the predicted photospheric flux, and interpret these signatures as evidence of debris disks in those systems. We combine this sample of FGK stars with similar published results to produce a sample of more than 350 main sequence AFGKM stars. The incidence of debris disks is 4.2(-1.1)(+2.0)% at 24 mu m for a sample of 213 Sun-like (FG) stars and 16.4(-2.9)(+2.8)% at 70 mu m for 225 Sun-like (FG) stars. We find that the excess rates for A, F, G, and K stars are statistically indistinguishable, but with a suggestion of decreasing excess rate toward the later spectral types; this may be an age effect. The lack of strong trend among FGK stars of comparable ages is surprising, given the factor of 50 change in stellar luminosity across this spectral range. We also find that the incidence of debris disks declines very slowly beyond ages of 1 billion years. C1 [Trilling, D. E.; Rieke, G. H.; Su, K. Y. L.; Stansberry, J. A.; Blaylock, M.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Bryden, G.; Beichman, C. A.; Stapelfeldt, K. R.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Beeman, J. W.; Haller, E. E.] Lawrence Berkeley Natl Lab, Div Mat Sci, Berkeley, CA 94720 USA. [Haller, E. E.] Univ Calif Berkeley, Dept Mat Sci & Engn, Berkeley, CA 94720 USA. RP Trilling, DE (reprint author), Univ Arizona, Steward Observ, 933 N Cherry Ave, Tucson, AZ 85721 USA. EM trilling@as.arizona.edu RI Stapelfeldt, Karl/D-2721-2012; OI Su, Kate/0000-0002-3532-5580 NR 70 TC 184 Z9 185 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 FEB 20 PY 2008 VL 674 IS 2 BP 1086 EP 1105 DI 10.1086/525514 PG 20 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 266RK UT WOS:000253454500035 ER PT J AU Padmanabhan, N Schlegel, DJ Finkbeiner, DP Barentine, JC Blanton, MR Brewington, HJ Gunn, JE Harvanek, M Hogg, DW Ivezic, Z Johnston, D Kent, SM Kleinman, SJ Knapp, GR Krzesinski, J Long, D Neilsen, EH Nitta, A Loomis, C Lupton, RH Roweis, S Snedden, SA Strauss, MA Tucker, DL AF Padmanabhan, Nikhil Schlegel, David J. Finkbeiner, Douglas P. Barentine, J. C. Blanton, Michael R. Brewington, Howard J. Gunn, James E. Harvanek, Michael Hogg, David W. Ivezic, Zeljko Johnston, David Kent, Stephen M. Kleinman, S. J. Knapp, Gillian R. Krzesinski, Jurek Long, Dan Neilsen, Eric H., Jr. Nitta, Atsuko Loomis, Craig Lupton, Robert H. Roweis, Sam Snedden, Stephanie A. Strauss, Michael A. Tucker, Douglas L. TI An improved photometric calibration of the sloan digital sky survey imaging data SO ASTROPHYSICAL JOURNAL LA English DT Article DE techniques : photometric ID LUMINOUS RED GALAXIES; LARGE MAGELLANIC CLOUD; DATA RELEASE; STANDARD STARS; CELESTIAL EQUATOR; SYSTEM; TELESCOPE; CATALOG; EXTINCTION; EMISSION AB We present an algorithm to photometrically calibrate wide-field optical imaging surveys, which simultaneously solves for the calibration parameters and relative stellar fluxes using overlapping observations. The algorithm decouples the problem of "relative'' calibrations from that of "absolute'' calibrations; the absolute calibration is reduced to determining a few numbers for the entire survey. We pay special attention to the spatial structure of the calibration errors, allowing one to isolate particular error modes in downstream analyses. Applying this to the SDSS imaging data, we achieve similar to 1% relative calibration errors across 8500 deg(2) in griz; the errors are similar to 2% for the u band. These errors are dominated by unmodeled atmospheric variations at Apache Point Observatory. These calibrations, dubbed "uber-calibration,'' are now public with SDSS Data Release 6 and will be a part of subsequent SDSS data releases. C1 [Padmanabhan, Nikhil; Schlegel, David J.] Lawrence Berkeley Natl Labs, Div Phys, Berkeley, CA 94720 USA. [Padmanabhan, Nikhil] Princeton Univ, Joseph Henry Labs, Princeton, NJ 08544 USA. [Schlegel, David J.; Finkbeiner, Douglas P.; Gunn, James E.; Johnston, David; Knapp, Gillian R.; Loomis, Craig; Lupton, Robert H.; Strauss, Michael A.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. [Finkbeiner, Douglas P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Barentine, J. C.] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA. [Barentine, J. C.; Brewington, Howard J.; Harvanek, Michael; Kleinman, S. J.; Krzesinski, Jurek; Long, Dan; Neilsen, Eric H., Jr.; Nitta, Atsuko; Loomis, Craig; Snedden, Stephanie A.] Apache Point Observ, Sunspot, NM 88349 USA. [Blanton, Michael R.; Hogg, David W.] NYU, Dept Phys, New York, NY 10003 USA. [Ivezic, Zeljko] Univ Washington, Dept Astron, Seattle, WA 98195 USA. [Johnston, David] Jet Prop Lab, Pasadena, CA 91109 USA. [Kent, Stephen M.; Neilsen, Eric H., Jr.; Tucker, Douglas L.] Fermilab Natl Accelerator Lab, Batavia, IL 60510 USA. [Kleinman, S. J.] Subaru Telescope, Hilo, HI 96720 USA. [Krzesinski, Jurek] Cracow Pedag Univ, Mt Suhora Observ, PL-30084 Krakow, Poland. [Nitta, Atsuko] Gemini Observ, Hilo, HI 96720 USA. [Roweis, Sam] Univ Toronto, Dept Comp Sci, Toronto, ON M5S 3G4, Canada. RP Padmanabhan, N (reprint author), Lawrence Berkeley Natl Labs, Div Phys, Berkeley, CA 94720 USA. EM npadmanabhan@lbl.gov RI Padmanabhan, Nikhil/A-2094-2012; OI Tucker, Douglas/0000-0001-7211-5729; Hogg, David/0000-0003-2866-9403 NR 54 TC 323 Z9 323 U1 0 U2 6 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 FEB 20 PY 2008 VL 674 IS 2 BP 1217 EP 1233 DI 10.1086/524677 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 266RK UT WOS:000253454500048 ER PT J AU Ghosh, KK Punsly, B AF Ghosh, Kajal K. Punsly, Brian TI The discovery of soft X-ray-loud broad absorption line quasars SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE accretion, accretion disks; black hole physics; galaxies : jets; quasars : absorption lines; quasars : general ID ACTIVE GALACTIC NUCLEI; ROSAT PSPC; EMISSION; GALAXIES; STARS; ULTRAVIOLET; SEPARATION AB It has been known for more than a decade that BALQSOs ( broad absorption line quasars) are highly attenuated in the X-ray regime compared to other quasars, especially in the soft band (< 1 keV). Using X-ray selection techniques, we have found "soft X-ray-loud" BALQSOs that, by definition, have soft X-ray (0.3 keV) to UV (3000) flux density ratios that are higher than typical non-BAL radio-quiet quasars. Our sample of three sources includes one LoBALQSO (low-ionization BALQSO), which is generally considered to be the most highly attenuated in X-rays. The three QSOs are the only known BALQSOs that have X-ray observations that are consistent with no intrinsic soft X-ray absorption. The existence of a large X-ray luminosity and the hard ionizing continuum that it presents to potential UV absorption gas is in conflict with the ionization states that are conducive to line-driving forces within BAL winds ( especially for the LoBALs). C1 [Ghosh, Kajal K.] NASA, George C Marshall Space Flight Ctr, Univ Space Res Assoc, Huntsville, AL 35812 USA. [Punsly, Brian] ICRANet, I-65100 Pescara, Italy. RP Ghosh, KK (reprint author), NASA, George C Marshall Space Flight Ctr, Univ Space Res Assoc, VP62, Huntsville, AL 35812 USA. EM brian.m.punsly@L-3com.com NR 23 TC 6 Z9 6 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD FEB 20 PY 2008 VL 674 IS 2 BP L69 EP L72 DI 10.1086/529138 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 291YW UT WOS:000255234500003 ER PT J AU Immler, S Modjaz, M Landsman, W Bufano, F Brown, PJ Milne, P Dessart, L Holland, ST Koss, M Pooley, D Kirshner, RP Filippenko, AV Panagia, N Chevalier, RA Mazzali, PA Gehrels, N Petre, R Burrows, DN Nousek, JA Roming, PWA Pian, E Soderberg, AM Greiner, J AF Immler, S. Modjaz, M. Landsman, W. Bufano, F. Brown, P. J. Milne, P. Dessart, L. Holland, S. T. Koss, M. Pooley, D. Kirshner, R. P. Filippenko, A. V. Panagia, N. Chevalier, R. A. Mazzali, P. A. Gehrels, N. Petre, R. Burrows, D. N. Nousek, J. A. Roming, P. W. A. Pian, E. Soderberg, A. M. Greiner, J. TI Swift and Chandra detections of supernova 2006jc: Evidence for interaction of the supernova shock with a circumstellar shell SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE circumstellar matter; supernovae : individual (SN 2006jc); X-rays : general; X rays : individual (SN 2006jc); X rays : ISM; ultraviolet : ISM ID TELESCOPE; GALAXY; STAR AB The peculiar Type Ib supernova (SN) 2006jc has been observed with the UV/Optical Telescope (UVOT) and X-Ray Telescope (XRT) on board the Swift observatory over a period of 19-183 days after the explosion. Signatures of interaction of the outgoing SN shock with dense circumstellar material (CSM) are detected, such as strong X-ray emission (L0.2-10 > 10(39) erg s(-1) ) and the presence of Mg II 2800 angstrom line emission visible in the UV spectra. In combination with a Chandra observation obtained on day 40 after the explosion, the X-ray light curve is constructed, which shows a unique rise of the X-ray emission by a factor of similar to 5 over a period of similar to 4 months, followed by a rapid decline. We interpret the unique X-ray and UV properties as a result of the SN shock interacting with a shell of material that was deposited by an outburst of the SN progenitor 2 years prior to the explosion. Our results are consistent with the explosion of a Wolf-Rayet star that underwent an episodic mass ejection qualitatively similar to those of luminous blue variable stars prior to its explosion. This led to the formation of a dense (similar to 10(7) cm(-3)) shell at a distance of similar to 10(16) cm from the site of the explosion, which expands with the WR wind at a velocity of 1300 +/- 300 km s(-1). C1 [Immler, S.; Landsman, W.; Bufano, F.; Holland, S. T.; Koss, M.; Gehrels, N.; Petre, R.] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA. [Immler, S.; Holland, S. T.] NASA, Goddard Space Flight Ctr, Ctr Res & Explorat Space Sci & Technol, Greenbelt, MD 20771 USA. [Immler, S.; Koss, M.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Modjaz, M.; Kirshner, R. P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Bufano, F.] Osserv Astron Padova, INAF, I-35122 Padua, Italy. [Brown, P. J.; Burrows, D. N.; Nousek, J. A.; Roming, P. W. A.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Milne, P.; Dessart, L.] Steward Observ, Tucson, AZ 85721 USA. [Holland, S. T.] Univ Space Res Assoc, Columbia, MD 21044 USA. [Pooley, D.; Filippenko, A. V.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Panagia, N.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Chevalier, R. A.] Univ Virginia, Dept Astron, Charlottesville, VA 22904 USA. [Mazzali, P. A.; Pian, E.] Osserv Astron Trieste, INAF, I-34131 Trieste, Italy. [Mazzali, P. A.] Max Planck Inst Astrophys, D-85741 Garching, Germany. [Soderberg, A. M.] CALTECH, Dept Astron, Pasadena, CA 91125 USA. [Greiner, J.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. RP Immler, S (reprint author), NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA. EM stefan.immler@nasa.gov RI Gehrels, Neil/D-2971-2012; Koss, Michael/B-1585-2015; OI Koss, Michael/0000-0002-7998-9581; Pian, Elena/0000-0001-8646-4858 NR 16 TC 40 Z9 40 U1 0 U2 3 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD FEB 20 PY 2008 VL 674 IS 2 BP L85 EP L88 DI 10.1086/529373 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 291YW UT WOS:000255234500007 ER PT J AU Sheeley, NR Herbst, AD Palatchi, CA Wang, YM Howard, RA Moses, JD Vourlidas, A Newmark, JS Socker, DG Plunkett, SP Korendyke, CM Burlaga, LF Davila, JM Thompson, WT St Cyr, OC Harrison, RA Davis, CJ Eyles, CJ Halain, JP Wang, D Rich, NB Battams, K Esfandiari, E Stenborg, G AF Sheeley, N. R., Jr. Herbst, A. D. Palatchi, C. A. Wang, Y. -M. Howard, R. A. Moses, J. D. Vourlidas, A. Newmark, J. S. Socker, D. G. Plunkett, S. P. Korendyke, C. M. Burlaga, L. F. Davila, J. M. Thompson, W. T. St Cyr, O. C. Harrison, R. A. Davis, C. J. Eyles, C. J. Halain, J. P. Wang, D. Rich, N. B. Battams, K. Esfandiari, E. Stenborg, G. TI Secchi observations of the Sun's garden-hose density spiral SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE Sun : corona; Sun : coronal mass ejections (CMEs); Sun : magnetic fields ID CORONA AB The SECCHI HI2 white-light imagers on the STEREO A and B spacecraft show systematically different proper motions of material moving outward from the Sun in front of high-speed solar wind streams from coronal holes. As a group of ejections enters the eastern (A) field of view, the elements at the rear of the group appear to overrun the elements at the front. (This is a projection effect and does not mean that the different elements actually merge.) The opposite is true in the western (B) field; the elements at the front of the group appear to run away from the elements at the rear. Elongation/ time maps show this effect as a characteristic grouping of the tracks of motion into convergent patterns in the east and divergent patterns in the west, consistent with ejections from a single longitude on the rotating Sun. Evidently, we are observing segments of the "garden-hose" spiral made visible when fast wind from a low-latitude coronal hole compresses blobs of streamer material being shed at the leading edge of the hole. C1 [Sheeley, N. R., Jr.; Herbst, A. D.; Palatchi, C. A.; Wang, Y. -M.; Howard, R. A.; Moses, J. D.; Vourlidas, A.; Newmark, J. S.; Socker, D. G.; Plunkett, S. P.; Korendyke, C. M.] USN, Res Lab, Div Space Sci, Washington, DC 20375 USA. [Burlaga, L. F.; Davila, J. M.; Thompson, W. T.; St Cyr, O. C.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Harrison, R. A.; Davis, C. J.; Eyles, C. J.] Rutherford Appleton Lab, Didcot OX11 0QX, Oxon, England. [Eyles, C. J.] Univ Birmingham, Sch Phys & Astron, Birmingham B15 2TT, W Midlands, England. [Halain, J. P.] Univ Liege, Ctr Spatiale Liege, B-4031 Angleur, Belgium. [Wang, D.; Rich, N. B.; Battams, K.; Esfandiari, E.] Interferometr Inc, Herndon, VA 20171 USA. [Stenborg, G.] Catholic Univ Amer, Washington, DC 20064 USA. RP Sheeley, NR (reprint author), USN, Res Lab, Div Space Sci, Washington, DC 20375 USA. EM sheeley@spruce.nrl.navy.mil RI Vourlidas, Angelos/C-8231-2009; Thompson, William/D-7376-2012; Scott, Christopher/H-8664-2012 OI Vourlidas, Angelos/0000-0002-8164-5948; Scott, Christopher/0000-0001-6411-5649 NR 5 TC 42 Z9 42 U1 0 U2 2 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD FEB 20 PY 2008 VL 674 IS 2 BP L109 EP L112 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 291YW UT WOS:000255234500013 ER PT J AU Wolf, S Schegerer, A Beuther, H Padgett, DL Stapelfeldt, KR AF Wolf, S. Schegerer, A. Beuther, H. Padgett, D. L. Stapelfeldt, K. R. TI Submillimeter structure of the disk of the Butterfly Star SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE circumstellar matter; planetary systems : formation; planetary systems : protoplanetary disks; radiative transfer; stars : individual (IRAS 04302+2247); submillimeter ID YOUNG STELLAR OBJECTS; PROTOPLANETARY DISK; RADIATIVE-TRANSFER; ORIGIN; ENVELOPES; TAURUS; ARRAY; GAP AB We present a spatially resolved 894 mm map of the circumstellar disk of the Butterfly Star in Taurus ( IRAS 04302 + 2247), obtained with the Submillimeter Array (SMA). The predicted and observed radial brightness profiles agree well in the outer disk region but differ in the inner region with an outer radius of similar to 80-120 AU. In particular, we find a local minimum of the radial brightness distribution at the center, which can be explained by an increasing density/optical depth combined with the decreasing vertical extent of the disk toward the center. Our finding indicates that young circumstellar disks can be optically thick at wavelengths as long as 894 mm. While earlier modeling lead to general conclusions about the global disk structure and, most importantly, evidence for grain growth in the disk ( Wolf, Padgett, & Stapelfeldt), the presented SMA observations provide more detailed constraints for the disk structure and dust grain properties in the inner, potentially planet-forming region (less than or similar to 80-120 AU) versus the outer disk region (similar to 120-300 AU). C1 [Wolf, S.] Univ Kiel, Inst Theoret Phys & Astrophys, D-24098 Kiel, Germany. [Wolf, S.; Schegerer, A.; Beuther, H.] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Padgett, D. L.] CALTECH, Pasadena, CA 91125 USA. [Stapelfeldt, K. R.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Wolf, S (reprint author), Univ Kiel, Inst Theoret Phys & Astrophys, Leibnizstr 15, D-24098 Kiel, Germany. EM swolf@mpia.de; schegerer@mpia.de; beuther@mpia.de; dlp@ipac.caltech.edu; krs@exoplanet.jpl.nasa.gov RI Stapelfeldt, Karl/D-2721-2012 NR 22 TC 15 Z9 16 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 FEB 20 PY 2008 VL 674 IS 2 BP L101 EP L104 DI 10.1086/529188 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 291YW UT WOS:000255234500011 ER PT J AU Minitti, ME Leshin, LA Dyar, MD Ahrens, TJ Guan, Y Luo, SN AF Minitti, Michelle E. Leshin, Laurie A. Dyar, M. Darby Ahrens, Thomas J. Guan, Yunbin Luo, Sheng-Nian TI Assessment of shock effects on amphibole water contents and hydrogen isotope compositions: 2. Kaersutitic amphibole experiments SO EARTH AND PLANETARY SCIENCE LETTERS LA English DT Article DE Mars; Martian meteorites; amphibole; impact shock; hydrogen isotopes ID IMPLANTED NOBLE-GASES; INDUCED DEVOLATILIZATION; MARTIAN METEORITE; FRACTIONATION; MANTLE; SERPENTINE; MINERALS; EXCHANGE; ROCKS AB To constrain the influence of impact shock on water and hydrogen isotope signatures of Martian meteorite kaersutites, we conducted shock recovery experiments on three terrestrial kaersutite crystals. Homogeneous impact shock to 32 GPa, commensurate with shock levels experienced by Martian meteorite kaersutites, led to increases in kaersutite water contents (Delta H2O-0.25-0.89 wt. %), decreases in Fe3+/Sigma Fe (4-20%), and enrichments in hydrogen isotope composition (Delta D=+66 to +87 parts per thousand) relative to pre-shock values. The latter values represent the largest shock-induced hydrogen isotope fractionations measured to date. These observations are explained most completely by a two-step shock process. First, shock-induced devolatilization led to hydrogen isotope enrichment through preferential loss of H relative to D. Second, reaction of the kaersutite with the ambient atmosphere led to increased water contents and reduced Fe. Fe reduction and water addition via the reaction Fe2+ + OH- <-> Fe3+ + O2- + 1/2H(2) explain the Fe3+/Sigma Fe data and some of the water data, Further water addition mechanisms (irreversible adsorption, shock implantation) are necessary to fully explain the increased water contents. Addition of water from the terrestrial atmosphere, which is isotopically light relative to the experimental kaersutite compositions, means the measured hydrogen isotope enrichments are likely minima. The measured (minimum) levels of hydrogen isotope enrichment are relevant to the hydrogen isotope variability within and among Martian kaersutites, but are minor relative to their absolute delta D values. Alternatively, addition of water from the enriched Martian atmosphere could explain both Martian kaersutite hydrogen isotope variability and absolute 6D values. However, the low Martian kaersutite water contents leave little room for significant water addition. The importance of the ambient atmosphere to the outcome of the shock experiments makes it difficult to translate our results to Mars given the unknown influence of its more tenuous atmosphere on the processes observed in the experiments. Our results suggest that shock is a feasible mechanism for influencing C1 [Minitti, Michelle E.] Arizona State Univ, Res Earth & Space Explorat, Ctr Meteorite Studies, Tempe, AZ 85287 USA. [Leshin, Laurie A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Dyar, M. Darby] Mt Holyoke Coll, Dept Astron, S Hadley, MA 01075 USA. [Ahrens, Thomas J.; Guan, Yunbin] CALTECH, Dept Geol & Planetary Sci, Pasadena, CA 91125 USA. [Luo, Sheng-Nian] Los Alamos Natl Lab, Los Alamos, NM 87545 USA. RP Minitti, ME (reprint author), Arizona State Univ, Res Earth & Space Explorat, Ctr Meteorite Studies, Tempe, AZ 85287 USA. EM minitti@asu.edu RI Luo, Sheng-Nian /D-2257-2010 OI Luo, Sheng-Nian /0000-0002-7538-0541 NR 29 TC 11 Z9 11 U1 0 U2 9 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0012-821X J9 EARTH PLANET SC LETT JI Earth Planet. Sci. Lett. PD FEB 20 PY 2008 VL 266 IS 3-4 BP 288 EP 302 DI 10.1016/j.epsl.2007.11.012 PG 15 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 271QC UT WOS:000253802800006 ER PT J AU Novak, MAM Watson, IM Delgado-Granados, H Rose, WI Cardenas-Gonzalez, L Realmuto, VJ AF Novak, M. A. Matiella Watson, I. M. Delgado-Granados, H. Rose, W. I. Cardenas-Gonzalez, L. Realmuto, V. J. TI Volcanic emissions from Popocatepetl volcano, Mexico, quantified using Moderate Resolution Imaging Spectroradiometer (MODIS) infrared data: A case study of the December 2000-January 2001 emissions SO JOURNAL OF VOLCANOLOGY AND GEOTHERMAL RESEARCH LA English DT Article DE Volcanic ash; SO(2); MODIS; infrared; Popocatepetl; remote sensing ID SULFUR-DIOXIDE EMISSIONS; KILAUEA VOLCANO; ASH CLOUDS; HAWAII; FLUX AB During December 2000 and January 2001, an increase in activity at Popocatepeti volcano, Mexico, was observed in both ground-based correlation spectrometer (COSPEC) data and in imagery from various satellite sensors, including the Moderate Resolution Imaging Spectroradiometer (MODIS), Total Ozone Mapping Spectrometer (TOMS), Advanced Very High Resolution Radiometer (AVHRR), and Geostationary Satellite 8 (GOES-8). Fine ash abundances detected by MODIS ranged between 6000 and 255,000 metric tons, and fine ash abundances detected by AVHRR, measured at different times, ranged between 4000 and 76,000 metric tons. The difference in ranges of ash mass detected by these two sensors depends largely on the difference in data acquisition time between the two sensors in detecting Popocatepetl's ash clouds. However, the difference could also be partly attributed to differences in spatial resolution and band sensitivity, which are believed to be significantly more favorable for MODIS. Mean effective radii for the two sensors images were typically within 10% of each other; values ranged from 5 to 8 pm and were strongly a function of residence time. Two types of infrared retrieval were used for the detection and quantification of SO(2) masses - one based on the 7.3 mu m SO(2) absorption feature and the other on the 8.6 mu m absorption feature. SO(2) values were attainable using the 8.6 mu m retrieval for most images, but were problematic using the 7.3 mu m retrieval. Only one SO(2) cloud was successfully measured by the 7.3 mu m retrieval (January 23rd 2001 04:50 UTC). This cloud was at an altitude of approximately 12 km, the highest cloud in the suite of images analyzed, and yielded an SO(2) mass of 16,500 metric tons. This suggests that elevated heights - above similar to 10 km - are required to negate the effects of atmospheric water vapor upon the 7.3 mu m retrieval at tropical latitudes. SO(2) clouds for which the 8.6 mu m retrieval was successful but 7.3 mu m was not were at heights between 6 and 10 km. Comparison of SO(2) retrievals obtained from MODIS images directly to COSPEC measurements was achieved by taking cross sections of the plume in the MODIS SO, maps. Wind data at the appropriate altitude can then be used to calculate fluxes comparable to those measured by COSPEC in units of tons day(-1). The fluxes calculated from the plume transects fell within the range of fluxes measured by the COSPEC, at 5-32 kT day(-1) and suggest more emissions in mid to late December, and lower emission rates throughout January. The MODIS data also complement a ground-based study on magnetic anomalies in which it was observed that more magma was extruded in the January 23, 2001 eruption than in the eruptions in December of 2000. Ash quantification from MODIS imagery suggests that the majority of fine ash was erupted in January of 2001. (C) 2007 Elsevier B.V. All rights reserved. C1 [Novak, M. A. Matiella; Watson, I. M.; Rose, W. I.] Michigan Technol Univ, Dept Geog & Min Engn & Sci, Houghton, MI 49931 USA. [Watson, I. M.] Univ Bristol, Dept Earth Sci, Bristol BS8 IRJ, Avon, England. [Delgado-Granados, H.] Univ Nacl Autonoma Mexico, Inst Geofis, Mexico City, DF, Mexico. [Cardenas-Gonzalez, L.] Ctr Nacl Prevenc Desastres, Coyoacan 04360, Mexico. [Realmuto, V. J.] Jet Prop Lab, Pasadena, CA 91109 USA. RP Novak, MAM (reprint author), Michigan Technol Univ, Dept Geog & Min Engn & Sci, 1400 Townsend Dr, Houghton, MI 49931 USA. EM mamatiel@mtu.edu RI Rose, William/A-7923-2009; Watson, Matt/E-5236-2011; Delgado Granados, Hugo/J-3056-2013 OI Watson, Matt/0000-0001-9198-2203; Delgado Granados, Hugo/0000-0001-5263-7968 NR 20 TC 8 Z9 8 U1 0 U2 9 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0377-0273 J9 J VOLCANOL GEOTH RES JI J. Volcanol. Geotherm. Res. PD FEB 20 PY 2008 VL 170 IS 1-2 BP 76 EP 85 DI 10.1016/j.jvolgeores.2007.09.010 PG 10 WC Geosciences, Multidisciplinary SC Geology GA 290FU UT WOS:000255109500008 ER PT J AU Awaki, H Anabuki, N Fukazawa, Y Gallo, LC Ikeda, S Isobe, N Itoh, T Kunieda, H Makishima, K Markowitz, A Miniutti, G Mizuno, T Okajima, T Ptak, A Reeves, JN Takahashi, T Terashima, Y Yaqoob, T AF Awaki, Hisamitsu Anabuki, Naohisa Fukazawa, Yasushi Gallo, Luigi C. Ikeda, Shinya Isobe, Naoki Itoh, Takeshi Kunieda, Hideyo Makishima, Kazuo Markowitz, Alex Miniutti, Giovanni Mizuno, Tsunefumi Okajima, Takashi Ptak, Andrew Reeves, James N. Takahashi, Tadayuki Terashima, Yuichi Yaqoob, Tahir TI Wide-band spectroscopy of the Compton thick Seyfert 2 galaxy Markarian 3 with Suzaku SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN LA English DT Article DE galaxies : active; galaxies : individual (Markarian 3); galaxies : Seyfert ID X-RAY-SPECTRUM; ACTIVE GALACTIC NUCLEI; NARROW-LINE REGION; BOARD SUZAKU; K-LINES; IRON; ABUNDANCES; ALPHA; SPECTROPOLARIMETRY; PHOTOIONIZATION AB We obtained a wide-band spectrum of the Compton-thick Seyfert 2 galaxy Mkn 3 with Suzaku. The observed spectrum was clearly resolved into weak, soft power-law emission, a heavily absorbed power-law component, cold reflection, and many emission lines. The heavily absorbed component, absorbed by gas with a column density of 1. 1 x 10(24) cm(-2), has an intrinsic 2-10 keV luminosity of similar to 1. 6 x 10(43) erg s(-1), and is considered to be direct emission from the Mkn 3 nucleus. The reflection component was interpreted as being the reflection of direct light off a cold, thick material; the reflection fraction, R, was 1.36 +/- 0.20. The cold material is inferred to be located > 1 pc from the central black hole of Mkn 3, due to the low ionization parameter of iron ( xi I erg cm s(-1)) and the narrow iron line width (sigma < 22 eV). The weak, soft power-law emission is considered to be scattered light by ionized gas with a scattering fraction of 0.9 +/- 0.2%. The existence of many highly ionized lines in the observed spectrum indicates that the ionized gas has a broad ionized structure, with xi = 10-1000 erg cm s(-1). This high-quality spectrum obtained by Suzaku can be considered to be a template for studies of Seyfert 2 galaxies. C1 [Awaki, Hisamitsu; Ikeda, Shinya; Terashima, Yuichi] Ehime Univ, Dept Phys, Matsuyama, Ehime 7908577, Japan. [Anabuki, Naohisa] Osaka Univ, Dept Earth & Space Sci, Osaka 5600043, Japan. [Fukazawa, Yasushi] Hiroshima Univ, Dept Phys Sci, Hiroshima 7398526, Japan. [Gallo, Luigi C.] Univ St Andrews, Sch Phys & Astron, SUPA, St Andrews KY16 9SS, Fife, Scotland. [Isobe, Naoki; Makishima, Kazuo] RIKEN, Wako, Saitama 3510198, Japan. [Itoh, Takeshi; Makishima, Kazuo] Univ Tokyo, Dept Phys, Bunkyo Ku, Tokyo 1130033, Japan. [Kunieda, Hideyo] Nagoya Univ, Dept Phys, Chikusa Ku, Nagoya, Aichi 4648602, Japan. [Markowitz, Alex; Okajima, Takashi; Ptak, Andrew; Reeves, James N.; Yaqoob, Tahir] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA. [Markowitz, Alex; Miniutti, Giovanni; Yaqoob, Tahir] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Miniutti, Giovanni] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. [Reeves, James N.] Univ Keele, Sch Phys & Geog Sci, Astrophys Grp, Keele ST5 5BG, Staffs, England. [Takahashi, Tadayuki] Japan Aerosp Explorat Agcy, Inst Space & Astronaut Sci, Sagamihara, Kanagawa 2298510, Japan. RP Awaki, H (reprint author), Ehime Univ, Dept Phys, Matsuyama, Ehime 7908577, Japan. EM awaki@astro.phys.sci.ehime-u.ac.jp RI Miniutti, Giovanni/L-2721-2014; XRAY, SUZAKU/A-1808-2009 OI Miniutti, Giovanni/0000-0003-0707-4531; NR 42 TC 26 Z9 26 U1 0 U2 1 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 FEB 20 PY 2008 VL 60 SI 1 BP S293 EP S305 DI 10.1093/pasj/60.sp1.S293 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 300IY UT WOS:000255818700029 ER PT J AU Bamba, A Fukazawa, Y Hiraga, JS Hughes, JP Katagiri, H Kokubun, M Koyama, K Miyata, E Mizuno, T Mori, K Nakajima, H Ozaki, M Petre, R Takahashi, H Takahashi, T Tanaka, T Terada, Y Uchiyama, Y Watanabe, S Yamaguch, H AF Bamba, Aya Fukazawa, Yasushi Hiraga, Junko S. Hughes, John P. Katagiri, Hideaki Kokubun, Motohide Koyama, Katsuji Miyata, Emi Mizuno, Tsunefumi Mori, Koji Nakajima, Hiroshi Ozaki, Masanobu Petre, Rob Takahashi, Hiromitsu Takahashi, Tadayuki Tanaka, Takaaki Terada, Yukikatsu Uchiyama, Yasunobu Watanabe, Shin Yamaguch, Hiroya TI Suzaku wide-band observations of SN 1006 SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN LA English DT Article DE acceleration of particles; ISM : individual (SN 1006); X-rays : ISM ID SUPERNOVA REMNANT SN-1006; X-RAY-DETECTOR; BOARD SUZAKU; PARTICLE-ACCELERATION; SHOCK ACCELERATION; ELECTRONS; EMISSION; MAXIMUM; CHANDRA; SN1006 AB We report on the wide-band spectra of SN 1006, as observed by Suzaku. Thermal and nonthermal emissions were successfully resolved thanks to the excellent spectral response of Suzaku's X-ray CCD XIS. The nonthermal emission could not be reproduced by a simple power-law model, but needed a roll-off at 5.7 x 10(16) Hz = 0.23 keV. The roll-off frequency is significantly higher in the northeastern rim than in the southwestern rim. We also placed the most stringent upper limit of the flux above 10 keV using the Hard X-ray Detector. C1 [Bamba, Aya; Ozaki, Masanobu; Takahashi, Tadayuki; Uchiyama, Yasunobu; Watanabe, Shin] Japan Aerosp Explorat Agcy, Inst Space & Astronaut Sci, Dept High Energy Astrophys, Sagamihara, Kanagawa 2298510, Japan. [Hiraga, Junko S.] RIKEN, Cosm Radiat Grp, Wako, Saitama 3510198, Japan. [Fukazawa, Yasushi; Katagiri, Hideaki] Hiroshima Univ, Dept Phys, Hiroshima 7398526, Japan. [Hughes, John P.] Rutgers State Univ, Dept Phys & Astron, Piscataway, NJ 08854 USA. [Koyama, Katsuji; Yamaguch, Hiroya] Kyoto Univ, Grad Sch Sci, Dept Phys, Kyoto 6068502, Japan. [Miyata, Emi; Nakajima, Hiroshi] Osaka Univ, Fac Sci, Dept Astrophys, Osaka 5600043, Japan. [Mori, Koji] Miyazaki Univ, Fac Engn, Dept Appl Phys, Miyazaki 8892192, Japan. [Petre, Rob] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Tanaka, Takaaki] Stanford Linear Accelerator Ctr, Menlo Pk, CA 94025 USA. [Terada, Yukikatsu] Saitama Univ, Sch Sci, Dept Phys, Saitama 3388570, Japan. RP Bamba, A (reprint author), Japan Aerosp Explorat Agcy, Inst Space & Astronaut Sci, Dept High Energy Astrophys, 3-1-1 Yoshinodai, Sagamihara, Kanagawa 2298510, Japan. EM bamba@astro.isas.jaxa.jp RI Terada, Yukikatsu/A-5879-2013; Ozaki, Masanobu/K-1165-2013; XRAY, SUZAKU/A-1808-2009 OI Terada, Yukikatsu/0000-0002-2359-1857; NR 40 TC 30 Z9 30 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 FEB 20 PY 2008 VL 60 SI 1 BP S153 EP S161 DI 10.1093/pasj/60.sp1.S153 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 300IY UT WOS:000255818700016 ER PT J AU Hyodo, Y Tsujimoto, M Hamaguchi, K Koyama, K Kitamoto, S Maeda, Y Tsuboi, Y Ezoe, Y AF Hyodo, Yoshiaki Tsujimoto, Masahiro Hamaguchi, Kenji Koyama, Katsuji Kitamoto, Shunji Maeda, Yoshitomo Tsuboi, Yohko Ezoe, Yuichiro TI Suzaku spectroscopy of extended X-ray emission in M 17 SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN LA English DT Article DE ISM : bubbles; ISM : HII regions; ISM : individual (M 17); X-rays : ISM ID HIGH-RESOLUTION; BOARD SUZAKU; VORONOI TESSELLATIONS; CORONAL ABUNDANCES; STELLAR OBJECTS; M17; CHANDRA; NEBULA; REGION; STARS AB We present the results of a Suzaku spectroscopic study of soft extended X-ray emission in the H II region of M 17. The spectrum of the extended emission was obtained with a high signal-to-noise ratio in a spatially resolved manner using the X-ray Imaging Spectrometer (XIS). We established that contamination by unresolved point sources, the Galactic Ridge X-ray emission, the cosmic X-ray background, and the local hot bubble emission is negligible in the background-subtracted XIS spectrum of the diffuse emission. Half a dozen emission lines were clearly resolved for the first time, including K alpha lines of highly ionized O, Ne, and Mg as well as L-series complex of Fe at 0.5-1.5keV. Based on diagnosis of these lines, we obtained the following results: (1) the extended emission is an optically thin thermal plasma, represented well by a single temperature of similar to 3.0 +/- 0.4 MK, (2) the abundances of elements with emission lines in the diffuse spectrum are 0.1-0.3 solar, while those of bright discrete sources are 0.3-1.5 solar, (3) the metal abundances relative to each other in the diffuse emission are consistent with solar, except for a Ne enhancement of a factor of similar to 2, (4) both the plasma temperature and the chemical composition of the diffuse emission show no spatial variation across the studied spatial scale of similar to 5 pc. C1 [Hyodo, Yoshiaki; Koyama, Katsuji] Kyoto Univ, Grad Sch Sci, Dept Phys, Kyoto 6068502, Japan. [Tsujimoto, Masahiro; Kitamoto, Shunji] Rikkyo Univ, Dept Phys, Tokyo 1718501, Japan. [Tsujimoto, Masahiro] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. NASA, Goddard Space Flight Ctr, Xray Astrophys Lab, Greenbelt, MD 20771 USA. CRESST, Greenbelt, MD 20771 USA. [Hamaguchi, Kenji] Univ Space Res Assoc, Columbia, MD 21044 USA. [Maeda, Yoshitomo] Japan Aerosp Explorat Agcy, Inst Space & Astronaut Sci, Sagamihara, Kanagawa 2298510, Japan. [Tsuboi, Yohko] Chuo Univ, Dept Sci & Engn, Bunkyo Ku, Tokyo 1128551, Japan. [Ezoe, Yuichiro] RIKEN, Cosm Radiat Lab, Wako, Saitama 3510198, Japan. RP Hyodo, Y (reprint author), Kyoto Univ, Grad Sch Sci, Dept Phys, Kita Shirakawa Oiwake Cho, Kyoto 6068502, Japan. EM hyodo@cr.scphys.kyoto-u.ac.jp RI XRAY, SUZAKU/A-1808-2009 NR 54 TC 15 Z9 15 U1 0 U2 1 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 FEB 20 PY 2008 VL 60 SI 1 BP S85 EP S93 DI 10.1093/pasj/60.sp1.S85 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 300IY UT WOS:000255818700009 ER PT J AU Itoh, T Done, C Makishima, K Madejski, G Awaki, H Gandhi, P Isobe, N Dewangan, GC Griffthis, RE Anabuki, N Okajima, T Reeves, JN Takahashi, T Ueda, Y Eguchi, S Yaqoob, T AF Itoh, Takeshi Done, Chris Makishima, Kazuo Madejski, Grzegorz Awaki, Hisamitsu Gandhi, Poshak Isobe, Naoki Dewangan, Gulab C. Griffthis, Richard E. Anabuki, Naohisa Okajima, Takashi Reeves, James N. Takahashi, Tadayuki Ueda, Yoshihiro Eguchi, Satohi Yaqoob, Tahir TI Suzaku wide-band X-ray spectroscopy of the Seyfert 2 AGN in NGC 4945 SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN LA English DT Article DE galaxies : active; galaxies : individual (NGC 4945); galaxies : Seyfert; X-rays : galaxies ID ACTIVE GALACTIC NUCLEI; NGC 4945; XMM-NEWTON; ASCA OBSERVATIONS; GALAXY NGC-4945; BOARD SUZAKU; EMISSION; SPECTRA; IRON; BEPPOSAX AB Suzaku observed a nearby Seyfert 2 galaxy, NGC 4945, which hosts one of the brightest active galactic nuclei above 20keV. Combining data from the two detectors aboard Suzaku, the AGN intrinsic nuclear emission and its reprocessed signals were observed simultaneously. The intrinsic emission is highly obscured with an absorbing column of similar to 5 X 10(24) CM-2. The spectrum below 10 keV is dominated by a reflection continuum and emission lines from neutral/ionized material. Along with a neutral iron K alpha line, a neutral iron K alpha line and a neutral nickel Ka line were detected for the first time from this source. The neutral lines and the cold reflection continuum are consistent with both originating in the same location. The Compton down-scattered shoulder in the neutral Fe-K alpha line is similar to 10% in flux of the narrow core, which confirms that the line originates from reflection, rather than transmission. The flux of the intrinsic emission varied by a factor of similar to 2 within similar to 20 ks, which requires the obscuring material to be geometrically thin. Broadband spectral modeling showed that the solid angle of the neutral reflector is less than a few x 10(-2) x 2 pi. All of this evidence regarding the reprocessed signals suggests that a disk-like absorber/reflector is viewed from a near edge-on angle. C1 [Itoh, Takeshi; Makishima, Kazuo] Univ Tokyo, Fac Sci, Dept Phys, Bunkyo Ku, Tokyo 1130033, Japan. [Done, Chris] Univ Durham, Dept Phys, Durham DH1 3LE, England. [Makishima, Kazuo; Gandhi, Poshak; Isobe, Naoki] RIKEN, Cosm Radiat Lab, Wako, Saitama 3510198, Japan. [Madejski, Grzegorz] Stanford Linear Accelerator Ctr, Menlo Pk, CA 94025 USA. [Awaki, Hisamitsu] Ehime Univ, Dept Phys & Astron, Matsuyama, Ehime 7908577, Japan. [Dewangan, Gulab C.; Griffthis, Richard E.] Carnegie Mellon Univ, Dept Phys, Pittsburgh, PA 15213 USA. [Anabuki, Naohisa] Osaka Univ, Dept Earth & Space Sci, Osaka 5600043, Japan. [Okajima, Takashi; Reeves, James N.] NASA, Goddard Space Flight Ctr, Explorat Universe Div, Greenbelt, MD 20771 USA. [Okajima, Takashi; Reeves, James N.; Yaqoob, Tahir] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Takahashi, Tadayuki] Japan Aerosp Explorat Agcy, Inst Space & Astronaut Sci, Sagamihara, Kanagawa 2298510, Japan. [Ueda, Yoshihiro; Eguchi, Satohi] Kyoto Univ, Dept Astron, Sakyo Ku, Kyoto 6068502, Japan. [Yaqoob, Tahir] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA. RP Itoh, T (reprint author), Univ Tokyo, Fac Sci, Dept Phys, Bunkyo Ku, 7-3-1 Hongo, Tokyo 1130033, Japan. EM titoh@amalthea.phys.s.u-tokyo.ac.jp RI XRAY, SUZAKU/A-1808-2009; done, chris/D-4605-2016 OI done, chris/0000-0002-1065-7239 NR 69 TC 37 Z9 37 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 FEB 20 PY 2008 VL 60 SI 1 BP S251 EP S261 DI 10.1093/pasj/60.sp1.S251 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 300IY UT WOS:000255818700026 ER PT J AU Markowitz, A Reeves, JN Miniutti, G Serlemitsos, P Kunieda, H Yaqoob, T Fabian, AC Fukazawa, Y Mushotzky, R Okajima, T Gallo, LC Awaki, H Griffiths, RE AF Markowitz, Alex Reeves, James N. Miniutti, Giovanni Serlemitsos, Peter Kunieda, Hideyo Yaqoob, Tahir Fabian, Andrew C. Fukazawa, Yasushi Mushotzky, Richard Okajima, Takashi Gallo, Luigi C. Awaki, Hisamitsu Griffiths, Richard E. TI The Suzaku observation of NGC 3516: Complex absorption and the broad and narrow FeK lines SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN LA English DT Article DE galaxies : active; galaxies : individual (NGC 3516); X-rays : galaxies ID ACTIVE GALACTIC NUCLEI; SEYFERT-GALAXY NGC-3516; X-RAY REFLECTION; XMM-NEWTON; EMISSION-LINE; BOARD SUZAKU; BLACK-HOLE; ACCRETION DISK; ALPHA PROFILE; COLD MATTER AB We present results from a 150 ks Suzaku observation of the Seyfert 1.5 NGC 3516 in 2005 October. The source was in a relatively highly absorbed state. Our best-fit model is consistent with the presence of a low-ionization absorber having a column density near 5 X 1022 cm(-2) and covering most of the X-ray continuum source (covering fraction 96-100%). A high-ionization absorbing component, which yields a narrow absorption feature consistent with Fe xxvi K, is confirmed. A relativistically broadened Fe K alpha line was required in all fits, even after the complex absorption was taken into account; an additional partial-covering component is an inadequate substitute for the continuum curvature associated with the broad Fe line. A narrow Fe Ka emission line has a velocity width consistent with the Broad Line Region. The low-ionization absorber may be responsible for producing the narrow Fe Ka line, though a contribution from additional material out of the line of sight is possible. We include in our model soft band emission lines from He- and H-like ions of N, O, Ne, and Mg, consistent with photo-ionization, though a small contribution from collisionally-ionized emission is possible. C1 [Markowitz, Alex; Reeves, James N.; Serlemitsos, Peter; Mushotzky, Richard; Okajima, Takashi] NASA, Goddard Space Flight Ctr, Xray Astrophys Lab, Greenbelt, MD 20771 USA. [Markowitz, Alex; Reeves, James N.; Yaqoob, Tahir; Okajima, Takashi] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Reeves, James N.] Univ Keele, Astrophys Grp, Sch Phys & Geog Sci, Keele ST5 5BG, Staffs, England. [Miniutti, Giovanni; Fabian, Andrew C.] Inst Astron, Cambridge CB3 0HA, England. [Kunieda, Hideyo] Nagoya Univ, Sch Sci, Dept Astrophys, Chikusa Ku, Nagoya, Aichi 4648602, Japan. [Kunieda, Hideyo] Japan Aerosp Explorat Agcy, Inst Space & Astronaut Sci, Sagamihara, Kanagawa 2298510, Japan. [Fukazawa, Yasushi] Hiroshima Univ, Dept Phys, Hiroshima 7398526, Japan. [Gallo, Luigi C.] Univ St Andrews, Sch Phys & Astron, SUPA, St Andrews KY16 9SS, Fife, Scotland. [Awaki, Hisamitsu] Ehime Univ, Fac Sci, Dept Phys, Matsuyama, Ehime 7908577, Japan. [Griffiths, Richard E.] Carnegie Mellon Univ, Dept Phys, Pittsburgh, PA 15213 USA. RP Markowitz, A (reprint author), NASA, Goddard Space Flight Ctr, Xray Astrophys Lab, Code 662, Greenbelt, MD 20771 USA. RI Miniutti, Giovanni/L-2721-2014; XRAY, SUZAKU/A-1808-2009 OI Miniutti, Giovanni/0000-0003-0707-4531; NR 65 TC 6 Z9 6 U1 0 U2 1 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 FEB 20 PY 2008 VL 60 SI 1 BP S277 EP S291 DI 10.1093/pasj/60.sp1.S277 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 300IY UT WOS:000255818700028 ER PT J AU Miller, ED Tsunemi, H Bautz, MW McCammon, D Fujimoto, R Hughes, JP Katsuda, S Kokubun, M Mitsuda, K Porter, FS Takei, Y Tsuboi, Y Yamasaki, NY AF Miller, Eric D. Tsunemi, Hiroshi Bautz, Mark W. McCammon, Dan Fujimoto, Ryuichi Hughes, John P. Katsuda, Satoru Kokubun, Motohide Mitsuda, Kazuhisa Porter, F. Scott Takei, Yoh Tsuboi, Yohko Yamasaki, Noriko Y. TI Suzaku observations of the North Polar Spur: Evidence for nitrogen enhancement SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN LA English DT Article DE ISM : abundances; ISM : individual (North Polar Spur); ISM : structure; ISM : supernova remnants; X-rays : ISM ID X-RAY-EMISSION; GALACTIC-CENTER; INTERSTELLAR-MEDIUM; LOOP-I; SCORPIO-CENTAURUS; SUPERNOVA REMNANT; STARBURST MODEL; CYGNUS LOOP; SOLAR-WIND; XMM-NEWTON AB We present observations of the North Polar Spur (NPS) using the X-ray Imaging Spectrometer (XIS) aboard the Suzaku X-ray satellite. The NPS is a large region of enhanced soft X-ray and radio emission projected above the plane of the Galaxy, likely produced by a series of supernovae and stellar winds from the nearby Sco-Cen OB association. The exceptional sensitivity and spectral resolution of the XIS below 1 keV allow unprecedented probing of low-energy spectral lines, including C VI (0.37 keV) and N VII (0.50 keV), and we have detected highly-ionized nitrogen toward the NPS for the first time. For this single pointing toward the brightest 3/4 keV emission (l = 26.degrees 8, b = +22.degrees 0), the best-fit NPS emission model implies a hot (kT approximate to 0.3 keV), collisional ionization equilibrium (CIE) plasma with depleted C, O, Ne, Mg, and Fe abundances of less than 0.5 solar, but an enhanced N abundance, with N/O = (4.0(-0.5)(+0.4)) times solar. The temperature and total thermal energy of the gas suggest heating by one or more supernovae, while the enhanced nitrogen abundance is best explained by enrichment from stellar material that has been processed by the CNO cycle. Due to the time required to develop AGB stars, we conclude that this N/O enhancement cannot be caused by the Sco-Cen OB association, but may result from a previous enrichment episode in the solar neighborhood. C1 [Miller, Eric D.; Bautz, Mark W.] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. [Tsunemi, Hiroshi; Katsuda, Satoru] Osaka Univ, Dept Earth & Space Sci, Osaka 5600043, Japan. [McCammon, Dan] Univ Wisconsin, Dept Phys, Madison, WI 53706 USA. [Fujimoto, Ryuichi; Mitsuda, Kazuhisa; Takei, Yoh; Yamasaki, Noriko Y.] Japan Aerosp Explorat Agcy, Inst Space & Astronaut Sci, Sagamihara, Kanagawa 2298510, Japan. [Hughes, John P.] Rutgers State Univ, Dept Phys & Astron, Piscataway, NJ 08854 USA. [Kokubun, Motohide] Univ Tokyo, Dept Phys, Bunkyo Ku, Tokyo 1130033, Japan. [Porter, F. Scott] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Takei, Yoh] SRON, NL-3584 CA Utrecht, Netherlands. [Tsuboi, Yohko] Chuo Univ, Dept Phys, Bunkyo Ku, Tokyo 1128551, Japan. RP Miller, ED (reprint author), MIT, Kavli Inst Astrophys & Space Res, 77 Massachusetts Ave, Cambridge, MA 02139 USA. EM milleric@mit.edu RI Yamasaki, Noriko/C-2252-2008; Mitsuda, Kazuhisa/C-2649-2008; Porter, Frederick/D-3501-2012; XRAY, SUZAKU/A-1808-2009 OI Porter, Frederick/0000-0002-6374-1119; NR 70 TC 14 Z9 14 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 FEB 20 PY 2008 VL 60 SI 1 BP S95 EP S106 DI 10.1093/pasj/60.sp1.S95 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 300IY UT WOS:000255818700010 ER PT J AU Ohno, M Fukazawa, Y Takahashi, T Yamaoka, K Sugita, S Pal'shin, V Frederiks, D Oleynik, P Ulanov, M Sakamoto, T Sato, G Hurley, K Tashiro, MS Urata, Y Onda, K Tamagawa, T Terada, Y Suzuki, M Soojing, H AF Ohno, Masanori Fukazawa, Yasushi Takahashi, Takuya Yamaoka, Kazutaka Sugita, Satoshi Pal'shin, Valentin Frederiks, Dmitry Oleynik, Philipp Ulanov, Mikhail Sakamoto, Takanori Sato, Goro Hurley, Kevin Tashiro, Makoto S. Urata, Yuji Onda, Kaori Tamagawa, Toru Terada, Yukikatsu Suzuki, Motoko Soojing, Hong TI Spectral properties of prompt emission of four short gamma-ray bursts observed by the Suzaku-WAM and the Konus-wind SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN LA English DT Article DE gamma rays : burst; gamma rays : observations ID ALL-SKY MONITOR; LIGHT CURVES; BOARD SUZAKU; CATALOG; HARD; GRB-050709; PERFORMANCE; AFTERGLOW; BEPPOSAX; DETECTOR AB We have performed a joint analysis of prompt emission from four bright short gamma-ray bursts (GRBs) with the Suzaku-WAM and the Konus-Wind experiments. This joint analysis allows us to investigate the spectral properties of short-duration bursts over a wider energy band with a higher accuracy. We find that these bursts have a high E-peak, around 1 MeV and have a harder power-law component than that of long GRBs. However, we can not determine whether these spectra follow the cut-off power-law model or the Band model. We also investigated the spectral lag, hardness ratio, inferred isotropic radiation energy and existence of a soft emission hump, in order to classify them into short or long GRBs using several criteria, in addition to the burst duration. We find that all criteria, except for the existence of the soft hump, support the fact that our four GRB samples are correctly classified as belonging to the short class. In addition, our broad-band analysis revealed that there is no evidence of GRBs with a very large hardness ratio, as seen in the BATSE short GRB sample, and that the spectral lag of our four short GRBs is consistent with zero, even in the MeV energy band, unlike long GRBs. Although our short GRB samples are still limited, these results suggest that the spectral hardness of short GRBs might not differ significantly from that of long GRBs, and also that the spectral lag at high energies could be a strong criterion for burst classification. C1 [Ohno, Masanori; Fukazawa, Yasushi; Takahashi, Takuya] Hiroshima Univ, Sch Sci, Dept Phys Sci, Hiroshima 7398526, Japan. [Yamaoka, Kazutaka; Sugita, Satoshi] Aoyama Gakuin Univ, Dept Math & Phys, Kanagawa 2298558, Japan. [Pal'shin, Valentin; Frederiks, Dmitry; Oleynik, Philipp; Ulanov, Mikhail] AF Ioffe Phys Tech Inst, Expt Astrophys Lab, St Petersburg 194021, Russia. [Sakamoto, Takanori; Sato, Goro] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Hurley, Kevin] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Tashiro, Makoto S.; Urata, Yuji; Onda, Kaori] Saitama Univ, Dept Phys, Sakura Ku, Saitama 3388570, Japan. [Tamagawa, Toru; Terada, Yukikatsu; Suzuki, Motoko] RIKEN, Wako, Saitama 3510198, Japan. [Soojing, Hong] Nihon Univ, Phys Lab, Coll Sci & Technol, Chiba 2748501, Japan. RP Ohno, M (reprint author), Hiroshima Univ, Sch Sci, Dept Phys Sci, 1-3-1 Kagamiyama, Hiroshima 7398526, Japan. EM ohno@hirax7.hepl.hiroshima-u.ac.jp RI Tashiro, Makoto/J-4562-2012; Terada, Yukikatsu/A-5879-2013; Oleynik, Philipp/C-1104-2014; Frederiks, Dmitry/C-7612-2014; Pal'shin, Valentin/F-3973-2014; Ulanov, Mikhail/B-3467-2015; XRAY, SUZAKU/A-1808-2009 OI Terada, Yukikatsu/0000-0002-2359-1857; Ulanov, Mikhail/0000-0002-0076-5228; NR 55 TC 11 Z9 11 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 FEB 20 PY 2008 VL 60 SI 1 BP S361 EP S373 DI 10.1093/pasj/60.sp1.S361 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 300IY UT WOS:000255818700035 ER PT J AU Smith, RK Mushotzky, R Mukai, K Kallman, T Markwardt, CB Tueller, J AF Smith, Randall K. Mushotzky, Richard Mukai, Koji Kallman, Tim Markwardt, Craig B. Tueller, Jack TI The symbiotic system SS73 17 seen with Suzaku SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN LA English DT Article DE stars : binaries : symbiotic; stars : individual (SS73 17); X-rays : stars ID EMISSION-LINE STARS; CH-CYGNI; VARIABLE-STARS; CATALOG; ASCA; DIAGNOSTICS; 4U-1954+319; SPECTRUM; BINARIES; SAMPLE AB We observed with Suzaku the symbiotic star SS73 17, motivated by the discovery by the INTEGRAL satellite and the Swift BAT survey that it emits hard X-rays. Our observations showed a highly-absorbed X-ray spectrum with N-H > 10(23) cm(-2), equivalent to A(v) > 26, although the source has B magnitude 11.3 and is also bright in UV. The source also shows strong, narrow iron lines including fluorescent Fe K as well as Fe xxv and Fe XXVI. The X-ray spectrum can be fit with a thermal model including an absorption component that partially covers the source. Most of the equivalent width of the iron fluorescent line in this model can be explained as a combination of reprocessing in a dense absorber plus reflection off a white dwarf surface, but it is likely that the continuum is partially seen in reflection as well. Unlike other symbiotic systems that show hard X-ray emission (CH Cyg, RT Cru, T CrB, GX 1+4), SS73 17 is not known to have shown nova-like optical variability, X-ray flashes, or pulsations, and has always shown faint soft X-ray emission. As a result, although it is likely a white dwarf, the nature of the compact object in SS73 17 is still uncertain. SS73 17 is probably an extreme example of the recently discovered and relatively small class of hard X-ray emitting symbiotic systems. C1 [Smith, Randall K.; Mushotzky, Richard; Kallman, Tim; Tueller, Jack] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Smith, Randall K.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. NASA, Goddard Space Flight Ctr, Xray Astrophys Lab, Greenbelt, MD 20771 USA. [Mukai, Koji] CRESST, Greenbelt, MD 20771 USA. [Mukai, Koji] Univ Maryland, Dept Phys, Baltimore, MD USA. [Markwardt, Craig B.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. RP Smith, RK (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. EM rsmith@milkway.gsfc.nasa.gov RI Tueller, Jack/D-5334-2012; XRAY, SUZAKU/A-1808-2009 NR 31 TC 3 Z9 3 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 FEB 20 PY 2008 VL 60 SI 1 BP S43 EP S48 DI 10.1093/pasj/60.sp1.S43 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 300IY UT WOS:000255818700005 ER PT J AU Takahashi, H Fukazawa, Y Mizuno, T Hirasawa, A Kitamoto, S Sudoh, K Cigita, T Kubota, A Makishima, K Itoh, T Parmar, AN Ebisawa, K Naik, S Dotani, T Kokubun, M Ohnuki, K Takahashi, T Yaqoob, T Angelini, L Ueda, Y Yamaoka, K Kotani, T Kawai, N Namiki, M Kohmura, T Negoro, H AF Takahashi, Hiromitsu Fukazawa, Yasushi Mizuno, Tsunefumi Hirasawa, Ayumi Kitamoto, Shunji Sudoh, Keisuke Cigita, Takayuki Kubota, Aya Makishima, Kazuo Itoh, Takeshi Parmar, Arvind N. Ebisawa, Ken Naik, Sachindra Dotani, Tadayasu Kokubun, Motohide Ohnuki, Kousuke Takahashi, Tadayuki Yaqoob, Tahir Angelini, Lorella Ueda, Yoshihiro Yamaoka, Kazutaka Kotani, Taro Kawai, Nobuyuki Namiki, Masaaki Kohmura, Takayoshi Negoro, Hitoshi TI Low/Hard state spectra of GRO J1655-40 observed with Suzaku SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN LA English DT Article DE accretion disks; black hole physics; stars : individual (GRO J1655-40); X-ray : binaries ID X-RAY-SPECTRA; ABSORPTION-LINE FEATURES; ACTIVE GALACTIC NUCLEI; CYGNUS X-1; BLACK-HOLE; SUPERLUMINAL SOURCE; 2005 OUTBURST; BOARD SUZAKU; ASCA OBSERVATIONS; MAGNETIC FLARES AB The Galactic black-hole binary GROJ1655-40, a source harboring superluminal jets, was observed with Suzaku on 2005 September 22-23. The source was detected over a broad and continuous energy range of 0.7-300 keV, with an intensity of similar to 50 mCrab at 20 keV At a distance of 3.2 kpc, the 0.7-300 keV luminosity was similar to 5.2 x 10(36) erg s(-1) (similar to 0.7% of the Eddington luminosity for a 6 M-circle dot black hole). The source was in a typical low/hard state, exhibiting a power-law shaped continuum with a photon index of similar to 1.6. During the observation, the source intensity gradually decreased by 25% at energies above similar to 3 keV, and by 35% below 2 keV. This, together with the soft X-ray spectra taken with the X-ray Imaging Spectrometer (XIS), suggests the presence of an independent soft component that can be represented by emission from a cool (similar to 0.2 keV) disk. The hard X-ray spectra obtained with the Hard X-ray Detector reveal a high-energy spectral cutoff, with an e-folding energy of similar to 200 keV. The entire 0.7-300 keV spectrum cannot be reproduced by a single thermal Comptonization model, even when considering reflection effects. Instead, the spectrum (except the soft excess) can be successfully explained by invoking two thermal-Comptonization components with different y-parameters. In contrast to the high/soft state spectra of this object, in which narrow iron absorption lines are detected with equivalent widths of 60-100 eV, the present XIS spectra bear no such features beyond an upper-limit equivalent width of 23 eV. C1 [Takahashi, Hiromitsu; Fukazawa, Yasushi; Mizuno, Tsunefumi; Hirasawa, Ayumi] Hiroshima Univ, Sch Sci, Dept Phys Sci, Hiroshima 7398526, Japan. [Kitamoto, Shunji; Sudoh, Keisuke; Cigita, Takayuki] Rikkyo Univ, Dept Phys, Toshima Ku, Tokyo 1718501, Japan. [Kubota, Aya] Shibaura Inst Technol, Dept Elect Informat Syst, Minami Ku, Saitama 3378570, Japan. [Makishima, Kazuo] RIKEN, Cosm Radiat Lab, Wako, Saitama 3510198, Japan. [Makishima, Kazuo; Itoh, Takeshi] Univ Tokyo, Dept Phys, Bunkyo Ku, Tokyo 1130033, Japan. [Parmar, Arvind N.] European Space Technol Ctr, European Space Agcy, Res & Sci Support Dept, Astrophys Miss Div, NL-2200 AG Noordwijk, Netherlands. [Ebisawa, Ken; Naik, Sachindra; Dotani, Tadayasu; Kokubun, Motohide; Ohnuki, Kousuke; Takahashi, Tadayuki] Japan Aerosp Explorat Agcy, Inst Space & Astronaut Sci, Sagamihara, Kanagawa 2298510, Japan. [Yaqoob, Tahir] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Angelini, Lorella] NASA, Goddard Space Flight Ctr, Explos Universe Div, Greenbelt, MD 20771 USA. [Ueda, Yoshihiro] Kyoto Univ, Dept Astron, Sakyo Ku, Kyoto 6068502, Japan. [Yamaoka, Kazutaka] Aoyama Gakuin Univ, Dept Math & Phys, Kanagawa 2298558, Japan. [Kotani, Taro; Kawai, Nobuyuki] Tokyo Inst Technol, Dept Phys, Meguro Ku, Tokyo 1528551, Japan. [Namiki, Masaaki] Osaka Univ, Grad Sch Sci, Dept Earth & Space Sci, Osaka 5600043, Japan. [Kohmura, Takayoshi] Kogakuin Univ, Dept Phys, Tokyo 1920015, Japan. [Negoro, Hitoshi] Nihon Univ, Coll Sci & Technol, Dept Phys, Chiyoda Ku, Tokyo 1018308, Japan. RP Takahashi, H (reprint author), Hiroshima Univ, Sch Sci, Dept Phys Sci, Hiroshima 7398526, Japan. EM hirotaka@hirax7.hepl.hiroshima-u.ac.jp RI XRAY, SUZAKU/A-1808-2009 NR 58 TC 38 Z9 38 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 FEB 20 PY 2008 VL 60 SI 1 BP S69 EP S83 DI 10.1093/pasj/60.sp1.S69 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 300IY UT WOS:000255818700008 ER PT J AU Takahashi, T Tanaka, T Uchiyama, Y Hiraga, JS Nakazawa, K Watanabe, S Bamba, A Hughes, JP Katagiri, H Kataoka, J Kokubun, M Koyama, K Mori, K Petre, R Takahashi, H Tsuboi, Y AF Takahashi, Tadayuki Tanaka, Takaaki Uchiyama, Yasunobu Hiraga, Junko S. Nakazawa, Kazuhiro Watanabe, Shin Bamba, Aya Hughes, John P. Katagiri, Hideaki Kataoka, Jun Kokubun, Motohide Koyama, Katsuji Mori, Koji Petre, Robert Takahashi, Hiromitsu Tsuboi, Yoko TI Measuring the broad-band X-ray spectrum from 400 eV to 40 keV in the southwest part of the supernova remnant RX J1713.7-3946 SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN LA English DT Article DE acceleration of particles; ISM : individual (RX J1713.7-3946); ISM : supernova remnants; X-rays : ISM ID DIFFUSIVE SHOCK ACCELERATION; MONTE-CARLO SIMULATOR; MAGNETIC-FIELD; BOARD SUZAKU; COSMIC-RAYS; HIGH-ENERGY; DETECTOR HXD; XMM-NEWTON; SHELL; EMISSION AB We report on results from Suzaku broadband X-ray observations of the southwest part of the galactic supernova remnant (SNR) RX J1713.7-3946 with an energy coverage of 0.4-40keV. The X-ray spectrum, presumably of synchrotron origin, is known to be completely lineless, making this SNR ideally suited for a detailed study of the X-ray spectral shape formed through efficient particle acceleration at high-speed shocks. With a sensitive hard X-ray measurement from the HXD PIN aboard Suzaku, we determined the hard X-ray spectrum in the 12-40 keV range to be described by a power law with photon index of Gamma = 3.2 +/- 0.2, significantly steeper than the soft X-ray index of Gamma = 2.4 +/- 0.05 measured previously with ASCA and other missions. We find that a simple power law fails to describe the full spectral range of 0.4-40 keV, and instead a power-law with an exponential cutoff with a hard index of Gamma = 1.50 +/- 0.09 and a high-energy cutoff of epsilon(c) = 1.2 +/- 0.3 keV formally provides an excellent fit over the full bandpass. If we use the so-called SRCUT model, as an alternative model, it gives a best-fit rolloff energy of epsilon(roll) = 0.95 +/- 0.04 keV. Together with the TeV gamma-ray spectrum, ranging from 0.3 to 100 TeV, recently obtained by HESS observations, our Suzaku observations of RX J1713.7-3946 provide stringent constraints on the highest-energy particles accelerated in a supernova shock. C1 [Takahashi, Tadayuki; Tanaka, Takaaki; Uchiyama, Yasunobu; Watanabe, Shin; Bamba, Aya; Kokubun, Motohide] Japan Aerosp Explorat Agcy, Inst Space & Astronaut Sci, Dept High Energy Astrophys, Sagamihara, Kanagawa 2298510, Japan. [Takahashi, Tadayuki; Nakazawa, Kazuhiro; Watanabe, Shin] Univ Tokyo, Dept Phys, Bunkyo Ku, Tokyo 1130033, Japan. [Tanaka, Takaaki] Stanford Linear Accelerator Ctr, Menlo Pk, CA 94025 USA. [Hiraga, Junko S.] RIKEN, Cosm Radiat Lab, Wako, Saitama 3510198, Japan. [Hughes, John P.] Rutgers State Univ, Dept Phys & Astron, Piscataway, NJ 08854 USA. [Katagiri, Hideaki; Takahashi, Hiromitsu] Hiroshima Univ, Dept Phys Sci, Hiroshima 7398526, Japan. [Koyama, Katsuji] Kyoto Univ, Dept Phys, Sakyo Ku, Kyoto 6068502, Japan. [Kataoka, Jun] Tokyo Inst Technol, Dept Phys, Meguro Ku, Tokyo 1528551, Japan. [Mori, Koji] Miyazaki Univ, Dept Appl Phys, Miyazaki 8892198, Japan. [Petre, Robert] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA. [Tsuboi, Yoko] Chuo Univ, Dept Phys, Bunkyo Ku, Tokyo 1128551, Japan. RP Takahashi, T (reprint author), Japan Aerosp Explorat Agcy, Inst Space & Astronaut Sci, Dept High Energy Astrophys, 3-1-1 Yoshinodai, Sagamihara, Kanagawa 2298510, Japan. RI XRAY, SUZAKU/A-1808-2009 NR 45 TC 32 Z9 32 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 FEB 20 PY 2008 VL 60 SI 1 BP S131 EP S140 DI 10.1093/pasj/60.sp1.S131 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 300IY UT WOS:000255818700014 ER PT J AU Yonetoku, D Tanabe, S Murakami, T Emura, N Aoyama, Y Kidamura, T Kodaira, H Kodama, Y Kozaka, R Nashimoto, T Okuno, S Yokota, S Yoshinari, S Abe, K Onda, K Tashiro, MS Urata, Y Nakagawa, YE Sugita, S Yamaoka, K Yoshida, A Ishimura, T Kawai, N Shimokawabe, T Kinugasa, K Kohmura, T Kubota, K Sugiyasu, K Ueda, Y Masui, K Nakazawa, K Takahashi, T Maeno, S Sonoda, E Yamauchi, M Kuwahara, M Tamagawa, T Matsuura, D Suzuki, M Barthelmy, S Gehrels, N Nousek, J AF Yonetoku, Daisuke Tanabe, Sachiko Murakami, Toshio Emura, Naomi Aoyama, Yuka Kidamura, Takashi Kodaira, Hironobu Kodama, Yoshiki Kozaka, Ryota Nashimoto, Takuro Okuno, Shinya Yokota, Satoshi Yoshinari, Satoru Abe, Keiichi Onda, Kaori Tashiro, Makoto S. Urata, Yuji Nakagawa, Yujin E. Sugita, Satoshi Yamaoka, Kazutaka Yoshida, Atsumasa Ishimura, Takuto Kawai, Nobuyuki Shimokawabe, Takashi Kinugasa, Kenzo Kohmura, Takayoshi Kubota, Kaori Sugiyasu, Kei Ueda, Yoshihiro Masui, Kensuke Nakazawa, Kazuhiro Takahashi, Tadayuki Maeno, Shouta Sonoda, Eri Yamauchi, Makoto Kuwahara, Makoto Tamagawa, Toru Matsuura, Daisuke Suzuki, Motoko Barthelmy, Scott Gehrels, Neil Nousek, John TI Spectral evolution of GRB 060904A observed with swift and Suzaku - Possibility of inefficient electron acceleration SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN LA English DT Article DE gamma rays : burst; radiation mechanisms : non-thermal; relativistic jet; X-rays : individual (GRB 060904A); X-rays : stars acceleration of particles ID GAMMA-RAY-BURSTS; BOARD SUZAKU; EMISSION; AFTERGLOWS; CATALOG; SHELLS AB We observed an X-ray afterglow of GRB 060904A with the Swift and Suzaku satellites. We found rapid spectral softening during both the prompt tail phase and the decline phase of an X-ray flare in the Swift/BAT and Swift/XRT +004 data. The observed spectra were fit by power-law photon indices which rapidly changed from Gamma = (+1.51)(-0.03) to Gamma = 5.30(-0.59)(+0.69) within a few hundred seconds. This is one of the steepest X-ray spectra ever observed, making it quite difficult to explain by simple electron-acceleration and synchrotron -radiation processes. We then applied an alternative broken power-law with exponential cutoff (BPEC) model. It is valid to consider the exponential shape is equivalent to a synchrotron cutoff. Since the spectral cutoff appears in the soft X-ray band, we conclude that the electron acceleration must be inefficient in the internal shocks of GRB 060904A. These cutoff spectra suddenly disappeared at the end of the prompt tail. After that, typical afterglow spectra with F = 2.0 have been continuously and preciously monitored by both Swift/XRT and Suzaku/XIS. We could successfully trace the temporal history of two characteristic break energies that have a time dependence of (proportional to t(-3)-t(-4), while the following afterglow spectra are quite stable. This fact indicates that the emitting material of the prompt tail is due to completely different dynamics from the shallow decay component. Therefore, the emission sites of two distinct phenomena obviously differ from each other. C1 [Yonetoku, Daisuke; Tanabe, Sachiko; Murakami, Toshio; Emura, Naomi; Aoyama, Yuka; Kidamura, Takashi; Kodaira, Hironobu; Kodama, Yoshiki; Kozaka, Ryota; Nashimoto, Takuro; Okuno, Shinya; Yokota, Satoshi; Yoshinari, Satoru] Kanazawa Univ, Dept Phys, Kanazawa, Ishikawa 9201192, Japan. [Abe, Keiichi; Onda, Kaori; Tashiro, Makoto S.; Urata, Yuji] Saitama Univ, Dept Phys, Sakura Ku, Saitama 3388570, Japan. [Nakagawa, Yujin E.; Sugita, Satoshi; Yamaoka, Kazutaka; Yoshida, Atsumasa] Aoyama Gakuin Univ, Dept Math & Phys, Kanagawa 2298551, Japan. [Ishimura, Takuto; Kawai, Nobuyuki; Shimokawabe, Takashi] Tokyo Inst Technol, Dept Phys, Meguro Ku, Tokyo 1528551, Japan. [Kinugasa, Kenzo] Gunma Astron Observ, Takayama, Gunma 3770702, Japan. [Kohmura, Takayoshi] Kogakuin Univ, Dept Phys, Tokyo 1920015, Japan. [Kubota, Kaori; Sugiyasu, Kei; Ueda, Yoshihiro] Kyoto Univ, Dept Astron, Sakyo Ku, Kyoto 6068502, Japan. [Masui, Kensuke; Nakazawa, Kazuhiro; Takahashi, Tadayuki] JAXA, Inst Space & Astronaut Sci, Kanagawa 2298510, Japan. [Maeno, Shouta; Sonoda, Eri; Yamauchi, Makoto] Miyazaki Univ, Miyazaki 8892192, Japan. [Kuwahara, Makoto; Tamagawa, Toru] RIKEN, Wako, Saitama 3510198, Japan. [Kuwahara, Makoto; Tamagawa, Toru] Tokyo Univ Sci, Dept Phys, Shinjyuku Ku, Tokyo 1628601, Japan. [Matsuura, Daisuke] Osaka Univ, Dept Phys, Osaka 5600043, Japan. [Suzuki, Motoko] Tsukuba Space Ctr, Tsukuba, Ibaraki 3058505, Japan. [Barthelmy, Scott; Gehrels, Neil] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Nousek, John] Penn State Univ, University Pk, PA 16802 USA. RP Yonetoku, D (reprint author), Kanazawa Univ, Dept Phys, Kanazawa, Ishikawa 9201192, Japan. EM yonetoku@astro.s.kanazawa-u.ac.jp RI Barthelmy, Scott/D-2943-2012; Gehrels, Neil/D-2971-2012; Tashiro, Makoto/J-4562-2012; XRAY, SUZAKU/A-1808-2009 NR 30 TC 0 Z9 0 U1 0 U2 1 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 FEB 20 PY 2008 VL 60 SI 1 BP S351 EP S360 DI 10.1093/pasj/60.sp1.S351 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 300IY UT WOS:000255818700034 ER PT J AU Cornet, C Davies, R AF Cornet, C. Davies, R. TI Use of MISR measurements to study the radiative transfer of an isolated convective cloud: Implications for cloud optical thickness retrieval SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID INDEPENDENT PIXEL APPROXIMATION; ADEOS-POLDER; PART I; RESOLUTION; STRATOCUMULUS; ALBEDO; VARIABILITY; RADIANCE; BIASES AB Radiative transfer simulations of an isolated deep convective cloud reconstructed with stereo-techniques from the Multiangle Imaging Spectroradiometer (MISR) are compared with the reflectances measured at the nine MISR viewing angles. The simulations were done using a three dimensional Monte Carlo model, in which ocean reflectance, aerosol and Rayleigh scattering were prescribed to match the surrounding clear-sky MISR measurements. Making reasonable assumptions regarding the vertical and horizontal distribution of the volume extinction coefficient, we were able to reproduce the MISR measurements with the 3D radiative calculations. While the uniqueness of the these distributions cannot be proven, they all lead to retrievals of much larger cloud optical thickness and cloud water content than for a 1D retrieval. Averaged over the cloud, the difference was a factor of about 3, rising to 9 locally. This is a consequence of horizontal photon transport that serves to highlight the inadequacy of 1D retrievals for the case of deep convective cloud. Concerning the internal cloud properties, we noticed the angular distribution of modeled radiances did not match the measured radiances when an ice crystal phase function was applied. Better estimates of the optical depths and water contents of deep convective clouds appear to be obtainable by integrating an estimate of the extinction coefficient over the vertical cloud extent (when this can assessed) than by attempting to invert the radiance measured from a single-angle view using 1D theory. C1 [Cornet, C.; Davies, R.] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. [Cornet, C.] Univ Sci & Tech Lille Flandres Artois, Opt Atmospher Lab, Villeneuve Dascq, France. [Davies, R.] Univ Auckland, Dept Phys, Auckland 1, New Zealand. RP Cornet, C (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. EM celine.cornet@loa.univ-lille1.fr RI Davies, Roger/D-4296-2009 OI Davies, Roger/0000-0002-2991-0409 NR 39 TC 7 Z9 7 U1 0 U2 8 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 FEB 19 PY 2008 VL 113 IS D4 AR D04202 DI 10.1029/2007JD008921 PG 11 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 267TF UT WOS:000253531400003 ER PT J AU Naoki, K Ukita, J Nishio, F Nakayama, M Comiso, JC Gasiewski, A AF Naoki, Kazuhiro Ukita, Jinro Nishio, Fumihiko Nakayama, Masashige Comiso, Josefino C. Gasiewski, Al TI Thin sea ice thickness as inferred from passive microwave and in situ observations SO JOURNAL OF GEOPHYSICAL RESEARCH-OCEANS LA English DT Article ID SATELLITE IMAGERY; OKHOTSK SEA; AMSR-E; VARIABILITY; FREQUENCIES; POLYNYAS; WINTER; WATER; SAR AB Microwave radiometric signals from sea ice strongly reflect physical conditions of a layer near the ice surface. This study examines the extent to which the relationships of thickness with brightness temperature and with emissivity hold for thin sea ice, approximately <0.2-0.3 m, and how those relationships may arise from changes in brine characteristics through modification of dielectric properties near the ice surface. In order to address these questions we made concurrent measurements of sea ice thickness in the Sea of Okhotsk from a ship and passive microwave radiometry from an over-flying aircraft. The results show that the brightness temperature and emissivity increase with thickness approximately within the thin ice for a frequency range of 10-37 GHz. The relationship is more pronounced at lower frequencies and at the horizontal polarization. We also established an empirical relationship between ice thickness and salinity in the layer near the ice surface from a field experiment, which qualitatively supports the idea that changes in the near-surface brine characteristics contribute to the observed thickness-brightness temperature/emissivity relationship. On the basis of our results, we conclude that for thin ice, passive microwave radiometric signals likely contain indirect information on ice thickness through the dependence of dielectric properties on brine, which provides a plausible and common explanation for previously proposed passive microwave thickness algorithms. C1 [Naoki, Kazuhiro; Ukita, Jinro; Nishio, Fumihiko] Chiba Univ, Grad Sch Sci & Technol, Chiba 9502181, Japan. [Naoki, Kazuhiro; Ukita, Jinro; Nishio, Fumihiko] Chiba Univ, Ctr Environm Remote Sensing, Chiba 9502181, Japan. [Nakayama, Masashige] Kushiro Childrens Museum, Kushiro, Hokkaido 0850017, Japan. [Comiso, Josefino C.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Gasiewski, Al] NOAA, Div Phys Sci, Earth Syst Res Lab, Boulder, CO 80305 USA. RP Naoki, K (reprint author), Chiba Univ, Grad Sch Sci & Technol, 1-33 Yayoi, Chiba 9502181, Japan. EM naoki@restaff.chiba-u.jp; jukita@env.sc.niigata-u.ac.jp; fnishio@faculty.chiba-u.jp; nakayama@kodomoyugakukan.jp; josefino.c.comiso@nasa.gov; al.gasiewski@noaa.gov NR 34 TC 13 Z9 13 U1 0 U2 3 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 FEB 19 PY 2008 VL 113 IS C2 AR C02S16 DI 10.1029/2007JC004270 PG 11 WC Oceanography SC Oceanography GA 267TN UT WOS:000253532200003 ER PT J AU Zwally, HJ Yi, DH Kwok, R Zhao, YH AF Zwally, H. Jay Yi, Donghui Kwok, Ron Zhao, Yunhe TI ICESat measurements of sea ice freeboard and estimates of sea ice thickness in the Weddell Sea SO JOURNAL OF GEOPHYSICAL RESEARCH-OCEANS LA English DT Article ID WINTER SNOW COVER; SOUTHERN-OCEAN; WAVELET ANALYSIS; GLAS ALTIMETRY; ROSS SEA; VARIABILITY; ANTARCTICA; MOTION; ROUGHNESS; SSM/I AB Sea ice freeboard heights in the Weddell Sea of Antarctica are derived from the Ice, Cloud, and Land Elevation Satellite (ICESat) laser altimeter measurements, which have a unique range precision to flat surfaces of 2 cm within 70 m footprints spaced at 172 m along track. Although elevations of flat surfaces can be obtained to an accuracy of similar to 10 cm (1 sigma) per footprint, direct determination of freeboard heights is precluded by errors in knowledge of the geoid and temporal variability of the ocean surface. Therefore freeboards are determined relative to an ocean reference level detected over areas of open water and very thin ice within the sea ice pack using an along-track filtering method. The open water/thin ice selections show good agreement in the combined analysis of ICESat segments and Envisat Synthetic Aperture Radar (SAR) imagery. The average residual between the ICESat-measured ocean level and the EGM96 geoid is 1.4 m. Estimates of snow depth on the sea ice from AMSR-E passive microwave data along with nominal densities of snow, water, and sea ice are used to estimate sea ice thickness. Four periods of ICESat data in May-June (fall) and October-November (late winter) of 2004 and 2005 between longitudes 298 degrees E and 360 degrees E are analyzed. In the fall the mean freeboards are 0.28 m in 2004 and 0.29 m in 2005, and the mean thicknesses are 1.33 m in 2004 and 1.52 m in 2005. In late winter the freeboards grew to 0.37 m in 2004 and 0.35 in 2005, and the thicknesses grew to 2.23 m in 2004 and 2.31 m in 2005. The interannual differences in freeboard are small, and the larger interannual change in estimated thickness mainly represents differences in the snow depth estimates. Seasonal changes in the spatial patterns of freeboard and thickness over the 4 months correlate with the expected circulation of sea ice in the Weddell Sea, as indicated by sea ice velocity fields. C1 [Zwally, H. Jay; Yi, Donghui] NASA, Goddard Space Flight Ctr, Cryospher Sci Branch, SGT Inc, Greenbelt, MD 20771 USA. [Kwok, Ron] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Zhao, Yunhe] NASA, Goddard Space Flight Ctr, Caelum Res Corp, Oceans Sci Branch, Greenbelt, MD 20771 USA. RP Zwally, HJ (reprint author), NASA, Goddard Space Flight Ctr, Cryospher Sci Branch, SGT Inc, Code 614-1, Greenbelt, MD 20771 USA. EM donghui.yi@nasa.gov RI Kwok, Ron/A-9762-2008 OI Kwok, Ron/0000-0003-4051-5896 NR 44 TC 75 Z9 80 U1 0 U2 14 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 FEB 19 PY 2008 VL 113 IS C2 AR C02S15 DI 10.1029/2007JC004284 PG 17 WC Oceanography SC Oceanography GA 267TN UT WOS:000253532200004 ER PT J AU Hudman, RC Murray, LT Jacob, DJ Millet, DB Turquety, S Wu, S Blake, DR Goldstein, AH Holloway, J Sachse, GW AF Hudman, R. C. Murray, L. T. Jacob, D. J. Millet, D. B. Turquety, S. Wu, S. Blake, D. R. Goldstein, A. H. Holloway, J. Sachse, G. W. TI Biogenic versus anthropogenic sources of CO in the United States SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID ATMOSPHERIC CHEMISTRY; CARBONYL-COMPOUNDS; EMISSIONS; FOREST; FORMALDEHYDE; ISOPRENE; OZONE; MODEL AB Aircraft observations of carbon monoxide (CO) from the ICARTT campaign over the eastern United States in summer 2004 ( July 1-August 15), interpreted with a global 3-D model of tropospheric chemistry (GEOS-Chem), show that the national anthropogenic emission inventory from the U. S. Environmental Protection Agency (93 Tg CO y(-1)) is too high by 60% in summer. Our best estimate of the CO anthropogenic source for the ICARTT period is 6.4 Tg CO, including 4.6 Tg from direct emission and 1.8 Tg CO from oxidation of anthropogenic volatile organic compounds (VOCs). The biogenic CO source for the same period from the oxidation of isoprene and other biogenic VOCs is 8.3 Tg CO, and is independently constrained by ICARTT observations of formaldehyde (HCHO). Anthropogenic emissions of CO in the U.S. have decreased to the point that they are now lower than the biogenic source in summer. C1 [Hudman, R. C.; Murray, L. T.; Jacob, D. J.; Wu, S.] Harvard Univ, Sch Engn & Appl Sci, Cambridge, MA 02139 USA. [Blake, D. R.] Univ Calif Irvine, Sch Phys Sci, Irvine, CA 92697 USA. [Goldstein, A. H.] Univ Calif Berkeley, Div Ecosyst Sci, Dept Environm Sci Policy & Management, Berkeley, CA 94720 USA. [Holloway, J.] NOAA OAR, Earth Syst Res Lab, Boulder, CO USA. [Millet, D. B.] Univ Minnesota, Dept Soil Water & Climate, St Paul, MN 55108 USA. [Sachse, G. W.] NASA, Langley Res Ctr, Div Atmospher Sci, Hampton, VA 23681 USA. [Turquety, S.] Univ Paris 06, IPSL, Serv Aeron, F-75252 Paris 05, France. RP Hudman, RC (reprint author), Harvard Univ, Sch Engn & Appl Sci, 29 Oxford St, Cambridge, MA 02139 USA. EM hudman@fas.harvard.edu; ltmurray@fas.harvard.edu; djacob@fas.harvard.edu; dbm@umn.edu; solene.turquety@aero.jussieu.fr; wu18@fas.harvard.edu; drblake@uci.edu; agoldstein@nature.berkeley.edu; john.s.holloway@noaa.gov; glen.w.sachse@nasa.gov RI Hudman, Rynda/C-6118-2009; Goldstein, Allen/A-6857-2011; Millet, Dylan/G-5832-2012; Holloway, John/F-9911-2012; Murray, Lee/F-2296-2014; Chem, GEOS/C-5595-2014 OI Goldstein, Allen/0000-0003-4014-4896; Holloway, John/0000-0002-4585-9594; Murray, Lee/0000-0002-3447-3952; NR 23 TC 72 Z9 72 U1 1 U2 20 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 FEB 16 PY 2008 VL 35 IS 4 AR L04801 DI 10.1029/2007GL032393 PG 5 WC Geosciences, Multidisciplinary SC Geology GA 263QT UT WOS:000253232300003 ER PT J AU Parkinson, CL Comiso, JC AF Parkinson, Claire L. Comiso, Josefino C. TI Antarctic sea ice parameters from AMSR-E data using two techniques and comparisons with sea ice from SSM/I SO JOURNAL OF GEOPHYSICAL RESEARCH-OCEANS LA English DT Article ID WEDDELL SEA; TIME-SERIES; MICROWAVE; TRENDS; WATER; SMMR AB Antarctic sea ice concentrations and extents, derived from the satellite passive microwave data of the Advanced Microwave Scanning Radiometer for the Earth Observing System (AMSR-E) are close but not identical depending on which of two major algorithms is used in the calculations. Overall, ice extents tend to be higher and ice concentrations lower when determined from the AMSR-E bootstrap algorithm (ABA) than when determined from the enhanced NASA team (NT2) algorithm, although the differences are within the algorithm error bars. Both algorithms obtain similar negative slopes for the lines of linear least squares fit through the short (4.5-year) AMSR-E data record available so far. When the ABA results are compared with results from the bootstrap algorithm applied over the same time period to data from the Special Sensor Microwave Imager (SSM/I), the two bootstrap results, from different satellites and different instruments, match even more closely than the ABA versus NT2 results from the same AMSR-E instrument. This is encouraging and is likely due to considerable effort to minimize the AMSR-E versus SSM/ I bootstrap differences, in consideration of extending the SSM/I record (which goes back to 1987) with the AMSR-E results. C1 [Parkinson, Claire L.; Comiso, Josefino C.] NASA, Goddard Space Flight Ctr, Cryospher Sci Branch, Greenbelt, MD 20771 USA. RP Parkinson, CL (reprint author), NASA, Goddard Space Flight Ctr, Cryospher Sci Branch, Code 614 1, Greenbelt, MD 20771 USA. EM claire.l.parkinson@nasa.gov RI Parkinson, Claire/E-1747-2012 OI Parkinson, Claire/0000-0001-6730-4197 NR 22 TC 8 Z9 9 U1 0 U2 6 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 FEB 16 PY 2008 VL 113 IS C2 AR C02S06 DI 10.1029/2007JC004253 PG 15 WC Oceanography SC Oceanography GA 263SD UT WOS:000253235900001 ER PT J AU Naeye, R AF Naeye, Robert TI Density's child SO NEW SCIENTIST LA English DT Article C1 NASAs Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA. RP Naeye, R (reprint author), NASAs Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA. NR 0 TC 0 Z9 0 U1 1 U2 1 PU REED BUSINESS INFORMATION LTD PI SUTTON PA QUADRANT HOUSE THE QUADRANT, SUTTON SM2 5AS, SURREY, ENGLAND SN 0262-4079 J9 NEW SCI JI New Sci. PD FEB 16 PY 2008 VL 197 IS 2643 BP 34 EP 35 DI 10.1016/S0262-4079(08)60420-0 PG 2 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 264CG UT WOS:000253262300030 ER PT J AU Pugel, DE Vispute, RD Hullavarad, SS Venkatesan, T Varughese, B AF Pugel, D. Elizabeth Vispute, R. D. Hullavarad, S. S. Venkatesan, T. Varughese, B. TI Compositional origin of surface roughness variations in air-annealed ZnO single crystals SO APPLIED SURFACE SCIENCE LA English DT Article DE ZnO; single crystal; surface morphology; air-annealing ID OXIDE SURFACES; STABILITY; HYDROGEN AB We directly investigated the chemical compositional origin of surface roughness variations in air-annealed ZnO single crystal samples for annealing temperatures up to 1000 degrees C. Atomic Force Microscopy (AFM) showed temperature-dependent changes in surface roughness and morphology, with a maximum in surface roughness of 2 nm found for samples annealed at 400 degrees C. The O(1s) line, measured by X-ray Photoelectron Spectroscopy (XPS) showed a maximum for Zn(OH)(2) and a minimum for off-stoichiometric ZnO at 400 degrees C; while the Zn(2p) peaks show an increase in slope at that temperature. These results indicate that the roughness arises from Zn diffusion and loss of surface oxygen. (c) 2007 Elsevier B.V. All rights reserved. C1 [Pugel, D. Elizabeth; Vispute, R. D.; Venkatesan, T.] Univ Maryland, Dept Phys, College Pk, MD 20742 USA. [Varughese, B.] Univ Maryland, Dept Mat Sci & Engn, College Pk, MD 20742 USA. [Hullavarad, S. S.] Univ Alaska, Off Elect Miniaturizat, Fairbanks, AK 99701 USA. RP Pugel, DE (reprint author), NASA, Goddard Space Flight Ctr, Detector Syst Branch, Greenbelt, MD 20771 USA. EM Diane.E.Pugel@nasa.gov RI Venkatesan, Thirumalai/E-1667-2013 NR 16 TC 11 Z9 11 U1 0 U2 5 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0169-4332 EI 1873-5584 J9 APPL SURF SCI JI Appl. Surf. Sci. PD FEB 15 PY 2008 VL 254 IS 8 BP 2220 EP 2223 DI 10.1016/j.apsusc.2007.07.206 PG 4 WC Chemistry, Physical; Materials Science, Coatings & Films; Physics, Applied; Physics, Condensed Matter SC Chemistry; Materials Science; Physics GA 277FN UT WOS:000254198200003 ER PT J AU Kolasinski, RD Polk, JE Goebel, D Johnson, LK AF Kolasinski, Robert D. Polk, James E. Goebel, Dan Johnson, Lee K. TI Carbon sputtering yield measurements at grazing incidence SO APPLIED SURFACE SCIENCE LA English DT Article DE sputtering; QCM; thin film; ion beam; carbon ID ENERGY-DEPENDENCE; MONATOMIC SOLIDS; ION-BOMBARDMENT AB In this investigation, carbon sputtering yields were measured experimentally at varying angles of incidence under Xe+ bombardment. The measurements were obtained by etching a coated quartz crystal microbalance (QCM) with a low energy ion beam. The material properties of the carbon targets were characterized with a scanning electron microscope (SEM) and Raman spectroscopy. C sputtering yields measured under Ar+ and Xe+ bombardment at normal incidence displayed satisfactory agreement with previously published data over an energy range of 200 eV-1 keV. For Xe+ ions, the dependence of the yields on angle of incidence theta was determined for 0 degrees <= theta <= 80 degrees. Over this range, an increase in C sputtering yield by a factor of 4.8 was observed, with the peak in yield occurring at 70 degrees. This is a much higher variation compared to Xe+ -> Mo yields under similar conditions, a difference that may be attributed to higher scattering of the incident particles transverse to the beam direction than in the case of Xe+! C. In addition, the variation of the yields with theta was not strongly energy dependent. Trapping of Xe in the surface was observed, in contrast to observations using the QCM technique with metallic target materials. Finally, target surface roughness was characterized using atomic force microscope measurements to distinguish between the effects of local and overall angle of incidence of the target. (c) 2007 Elsevier B. V. All rights reserved. C1 [Kolasinski, Robert D.] CALTECH, Pasadena, CA 91125 USA. [Polk, James E.; Goebel, Dan; Johnson, Lee K.] CALTECH, Jet Prop Lab, NASA, Pasadena, CA 91109 USA. RP Kolasinski, RD (reprint author), Sandia Natl Labs, POB 969,MS 9161, Livermore, CA 94551 USA. EM rkolasi@sandia.gov NR 28 TC 14 Z9 14 U1 1 U2 6 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 FEB 15 PY 2008 VL 254 IS 8 BP 2506 EP 2515 DI 10.1016/j.apsusc.2007.09.082 PG 10 WC Chemistry, Physical; Materials Science, Coatings & Films; Physics, Applied; Physics, Condensed Matter SC Chemistry; Materials Science; Physics GA 277FN UT WOS:000254198200048 ER PT J AU Echer, E Gonzalez, WD Tsurutani, BT AF Echer, E. Gonzalez, W. D. Tsurutani, B. T. TI Interplanetary conditions leading to superintense geomagnetic storms (Dst <=-250 nT) during solar cycle 23 SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID MAGNETIC STORMS; INTENSE; DST; GEOEFFECTIVENESS; CRITERIA; MAXIMUM; CLOUDS AB The interplanetary causes of superintense geomagnetic storms (superstorms, Dst <= -250 nT) that occurred during solar cycle 23 are studied. Eleven superstorms occurred during the cycle, five close to solar maximum (2000-2001) and six in the post-maximum/declining phase (2003-2004). About 1/3 of the superstorms were caused by magnetic clouds (MCs), 1/3 by a combination of sheath and MC fields, and 1/3 by sheath fields alone. The interplanetary parameter best correlated with peak Dst was the time-integrated E(y) during the storm main phase (in contrast with peak B(s) and/or peak E(y) for less intense geomagnetic storms). The range of peak Dst for these storms was -263 to -422 nT. The storm main phase durations had a range of 3-33 h. We conclude from this study that: (1) only MCs and/or interplanetary sheaths had fields intense enough and with long enough durations to cause superstorms; (2) superstorms occurred only in the maximum and declining phases; (3) the total energy transferred from the solar wind to the magnetosphere is best correlated with the time-integrated solar wind E(y) parameter. C1 [Echer, E.; Gonzalez, W. D.] Inst Nacl Pesquisas Espaciais, BR-12227010 Sao Jose Dos Campos, Brazil. [Tsurutani, B. T.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Echer, E (reprint author), Inst Nacl Pesquisas Espaciais, CP 515,Avenida Asrtonautas 1758, BR-12227010 Sao Jose Dos Campos, Brazil. EM eecher@dge.inpe.br NR 25 TC 51 Z9 54 U1 0 U2 2 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 FEB 15 PY 2008 VL 35 IS 6 AR L06S03 DI 10.1029/2007GL031755 PG 5 WC Geosciences, Multidisciplinary SC Geology GA 263QV UT WOS:000253232500001 ER PT J AU Logan, JA Megretskaia, I Nassar, R Murray, LT Zhang, L Bowman, KW Worden, HM Luo, M AF Logan, Jennifer A. Megretskaia, Inna Nassar, Ray Murray, Lee T. Zhang, Lin Bowman, Kevin W. Worden, Helen M. Luo, Ming TI Effects of the 2006 El Nino on tropospheric composition as revealed by data from the Tropospheric Emission Spectrometer (TES) SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID OZONE AB The Tropospheric Emission Spectrometer (TES) is unique in providing multi-year coincident tropospheric profiles of CO, O(3) and H(2)O. TES data show large differences in these gases over Indonesia and the eastern Indian Ocean in October-December 2006 relative to 2005. In 2006, O3 was higher by 15-30 ppb (30-75%) while CO was higher by > 80 ppb in October and November, and by similar to 25 ppb in December. These differences were caused by high fire emissions from Indonesia in 2006 associated with the lowest rainfall since 1997, reduced convection during the moderate El Nino, and reduced photochemical loss because of lower H2O. The persistence of the O3 difference into December is consistent with higher NO(x) emissions from lightning in 2006. TES CO and O3 enhancements in 2006 were larger than those observed during the weak El Nino of 2004. C1 [Logan, Jennifer A.; Megretskaia, Inna; Nassar, Ray; Murray, Lee T.] Harvard Univ, Sch Engn & Appl Sci, Cambridge, MA 02138 USA. [Bowman, Kevin W.; Luo, Ming] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Worden, Helen M.] Natl Ctr Atmospher Res, Div Atmospher Chem, Boulder, CO 80305 USA. [Zhang, Lin] Harvard Univ, Dept Earth & Planetary Sci, Cambridge, MA 02138 USA. RP Logan, JA (reprint author), Harvard Univ, Sch Engn & Appl Sci, 29 Oxford St, Cambridge, MA 02138 USA. EM jlogan@seas.harvard.edu RI Zhang, Lin/A-6729-2008; Murray, Lee/F-2296-2014; Zhang, Lin/H-9801-2014; OI Zhang, Lin/0000-0003-2383-8431; Murray, Lee/0000-0002-3447-3952; Nassar, Ray/0000-0001-6282-1611 NR 26 TC 77 Z9 79 U1 1 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 FEB 15 PY 2008 VL 35 IS 3 AR L03816 DI 10.1029/2007GL031698 PG 5 WC Geosciences, Multidisciplinary SC Geology GA 263QQ UT WOS:000253232000002 ER PT J AU Canovas, CR Hubbard, CG Olias, M Nieto, JM Black, S Coleman, ML AF Canovas, C. R. Hubbard, C. G. Olias, M. Nieto, J. M. Black, S. Coleman, M. L. TI Hydrochemical variations and contaminant load in the Rio Tinto (Spain) during flood events SO JOURNAL OF HYDROLOGY LA English DT Article DE AMD; Rio Tinto; metal load; flood events ID ACID-MINE DRAINAGE; IBERIAN PYRITE BELT; TRACE-METAL ENRICHMENTS; SOUTH-WEST SPAIN; SOUTHWESTERN SPAIN; SULFATE MINERALS; ESTUARINE SYSTEM; IRON-MOUNTAIN; SW SPAIN; RIVER AB The aim of this work is to study the hydrochemical variations during flood events in the Rio Tinto, SW Spain. Three separate rainfall/flood events were monitored in October 2004 following the dry season. In general, concentrations markedly increased following the first event (Fe from 99 to 1130 mg/L; Q(max) = 0.78 m(3)/s) while dissolved loads peaked in the second event (Fe = 7.5 kg/s, Cu = 0.83 kg/s, Zn = 0.82 kg/s; Q(max) = 77 m(3)/s) and discharge in the third event (Q(max) = 127 m(3)/s). This pattern reflects a progressive depletion of metals and sulphate stored in the dry summer as soluble evaporitic salt minerals and concentrated pore fluids, with dilution by freshwater becoming increasingly dominant as the month progressed. Variations in relative concentrations were attributed to oxyhydroxysulphate Fe precipitation, to relative changes in the sources of acid mine drainage (e.g. salt minerals, mine tunnels, spoil heaps etc.) and to differences in the rainfall distributions along the catchment. The contaminant load carried by the river during October 2004 was enormous, totalling some 770 t of Fe, 420 t of Al, 100 t of Cu, 100 t of Zn and 71 t of Mn. This represents the largest recorded example of this flush-out process in an acid mine drainage setting. Approximately 1000 times more water and 1408 200 times more dissolved elements were carried by the river during October 2004 than during the dry, low-flow conditions of September 2004, highlighting the key role of flood Events in the annual pollutant transport budget of semi-arid and and systems and the need to monitor these events in detail in order to accurately quantify pollutant transport. (c) 2007 Elsevier B.V. All rights reserved. C1 [Canovas, C. R.; Olias, M.] Univ Huelva, Dept Geodynam & Paleontol, Huelva 21071, Spain. [Hubbard, C. G.; Black, S.; Coleman, M. L.] Univ Reading, Sch Human & Environm Sci, Reading RG6 6AB, Berks, England. [Nieto, J. M.] Univ Huelva, Dept Geol, Huelva 21007, Spain. [Coleman, M. L.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. EM carlos.ruiz@dgeo.uhu.es RI Coleman, Max/A-1303-2007; Black, Stuart/A-1099-2014; Hubbard, Christopher/J-6150-2014; Olias, Manuel/O-5449-2014; Nieto, Jose Miguel/K-1935-2014; OI Coleman, Max/0000-0002-5514-1826; Black, Stuart/0000-0003-1396-4821; Hubbard, Christopher/0000-0002-8217-8122; Olias, Manuel/0000-0001-5394-3449; Nieto, Jose Miguel/0000-0002-0086-252X; RUIZ CANOVAS, CARLOS/0000-0002-2860-5154 NR 64 TC 55 Z9 55 U1 0 U2 16 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0022-1694 J9 J HYDROL JI J. Hydrol. PD FEB 15 PY 2008 VL 350 IS 1-2 BP 25 EP 40 DI 10.1016/j.jhydrol.2007.11.022 PG 16 WC Engineering, Civil; Geosciences, Multidisciplinary; Water Resources SC Engineering; Geology; Water Resources GA 268SR UT WOS:000253600200003 ER PT J AU Barrie, RL Gabb, TP Telesman, J Kantzos, PT Prescenzi, A Biles, T Bonacuse, PJ AF Barrie, R. L. Gabb, T. P. Telesman, J. Kantzos, P. T. Prescenzi, A. Biles, T. Bonacuse, P. J. TI Effectiveness of shot peening in suppressing fatigue cracking at non-metallic inclusions in Udimet (R) 720 SO MATERIALS SCIENCE AND ENGINEERING A-STRUCTURAL MATERIALS PROPERTIES MICROSTRUCTURE AND PROCESSING LA English DT Article DE shot peening; fatigue; inclusions; superalloy; disk AB The fatigue lives of modem powder metallurgy disk alloys can be reduced over an order of magnitude by cracking at inherent non-metallic inclusions. The objective of this work was to study the effectiveness of shot peening in suppressing LCF crack initiation and growth at surface non-metallic inclusions. Inclusions were carefully introduced at elevated levels during powder metallurgy processing of the nickel-base disk superalloy Udimet (R) 720. Multiple strain-controlled fatigue tests were then performed on machined specimens with and without shot peened test sections at 427 and 650 degrees C. The low cycle fatigue lives and failure initiation sites varied as functions of inclusion content, shot peening, and fatigue conditions. A large majority of the failures in as-machined specimens with the introduced inclusions occurred at cracks initiating from inclusions intersecting the specimen surface. These inclusions reduced fatigue life by up to 100x, when compared to lives of material without inclusions residing at specimen surface. Large inclusions produced the greatest reductions in life for tests at low strain ranges and high strain ratios. Shot peening improved life in many cases by reducing the most severe effects of inclusions. (C) 2007 Elsevier B.V. All rights reserved. C1 [Gabb, T. P.; Telesman, J.] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. [Barrie, R. L.] USA Aviat & Missile Command, Redstone Arsenal, AL 35895 USA. [Kantzos, P. T.] Honeywell Engine Syst, Phoenix, AZ 85038 USA. [Prescenzi, A.] Ohio State Univ, Columbus, OH 43210 USA. [Biles, T.] Alcoa Wheel & Forged Prod, Cleveland, OH 44105 USA. [Bonacuse, P. J.] NASA GRC, Army Res Lab, Cleveland, OH 44135 USA. RP Gabb, TP (reprint author), NASA, Glenn Res Ctr, 21000 Brookpk Rd, Cleveland, OH 44135 USA. EM timothy.p.gabb@nasa.gov NR 18 TC 13 Z9 15 U1 0 U2 8 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 FEB 15 PY 2008 VL 474 IS 1-2 BP 71 EP 81 DI 10.1016/j.msea.2007.03.100 PG 11 WC Nanoscience & Nanotechnology; Materials Science, Multidisciplinary; Metallurgy & Metallurgical Engineering SC Science & Technology - Other Topics; Materials Science; Metallurgy & Metallurgical Engineering GA 260SK UT WOS:000253030500009 ER PT J AU Raj, SV Ghosn, LJ AF Raj, S. V. Ghosn, L. J. TI Failure maps for rectangular 17-4PH stainless steel sandwiched foam panels SO MATERIALS SCIENCE AND ENGINEERING A-STRUCTURAL MATERIALS PROPERTIES MICROSTRUCTURE AND PROCESSING LA English DT Article DE 17-4PH; stainless steel; metallic foams; sandwiched foam panel; theoretical failure maps; design ID MECHANICAL-BEHAVIOR; CELLULAR MATERIALS; METAL FOAMS; IMPERFECTIONS; STIFFNESS; FRACTURE; SOLIDS; CREEP; CORES; BEAMS AB A new and innovative concept is proposed for designing lightweight fan blades for aircraft engines using commercially available 17-4PH precipitation hardened stainless steel. Rotating fan blades in aircraft engines experience a complex loading state consisting of combinations of centrifugal, distributed pressure and torsional loads. Theoretical failure plastic collapse maps, showing plots of the foam relative density versus face sheet thickness, t, normalized by the fan blade span length, L, have been generated for rectangular 17-4PH sandwiched foam panels under these three loading modes assuming three failure plastic collapse modes. These maps show that the 17-4PH sandwiched foam panels can fail by either the yielding of the face sheets, yielding of the foam core or wrinkling of the face sheets depending on foam relative density, the magnitude of t/L and the loading mode. The design envelop of a generic fan blade is superimposed on the maps to provide valuable insights on the probable failure modes in a sandwiched foam fan blade. Published by Elsevier B.V. C1 [Raj, S. V.] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. [Ghosn, L. J.] Ohio Aerosp Inst, Cleveland, OH 44135 USA. RP Raj, SV (reprint author), NASA, Glenn Res Ctr, MS 106-5,21000 Brookpk Rd, Cleveland, OH 44135 USA. EM sai.v.raj@nasa.gov NR 31 TC 8 Z9 8 U1 0 U2 6 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 FEB 15 PY 2008 VL 474 IS 1-2 BP 88 EP 95 DI 10.1016/j.msea.2007.03.102 PG 8 WC Nanoscience & Nanotechnology; Materials Science, Multidisciplinary; Metallurgy & Metallurgical Engineering SC Science & Technology - Other Topics; Materials Science; Metallurgy & Metallurgical Engineering GA 260SK UT WOS:000253030500011 ER PT J AU Jackson, TJ Moran, MS O'Neill, PE AF Jackson, T. J. Moran, M. S. O'Neill, P. E. TI Introduction to Soil Moisture Experiments 2004 (SMEX04) Special Issue SO REMOTE SENSING OF ENVIRONMENT LA English DT Editorial Material C1 [Jackson, T. J.; Moran, M. S.] USDA ARS, Washington, DC 20250 USA. [O'Neill, P. E.] NASA, Goddard Space Flight Ctr, Washington, DC 20546 USA. RP Jackson, TJ (reprint author), USDA ARS, Washington, DC 20250 USA. EM tjackson@hydrolab.ars.usda.gov NR 12 TC 15 Z9 16 U1 2 U2 6 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 FEB 15 PY 2008 VL 112 IS 2 BP 301 EP 303 DI 10.1016/j.rse.2007.01.021 PG 3 WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic Technology SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science & Photographic Technology GA 261GW UT WOS:000253068100001 ER PT J AU Yilmaz, MT Hunt, ER Goins, LD Ustin, SL Vanderbilt, VC Jackson, TJ AF Yilmaz, M. Tugrul Hunt, E. Raymond, Jr. Goins, Lyssa D. Ustin, Susan L. Vanderbilt, Vern C. Jackson, Thomas J. TI Vegetation water content during SMEX04 from ground data and Landsat 5 Thematic Mapper imagery SO REMOTE SENSING OF ENVIRONMENT LA English DT Article DE decision tree classification; equivalent water thickness; leaf area index; normalized difference infrared index; Soil Moisture Experiment 2004 ID LEAF-AREA INDEX; DECISION TREE CLASSIFICATION; REMOTELY-SENSED DATA; ATMOSPHERIC CORRECTION; REFLECTANCE DATA; FUEL MOISTURE; LIQUID WATER; LAND-COVER; MODIS; SOIL AB Vegetation water content is an important parameter for retrieval of soil moisture from microwave data and for other remote sensing applications. Because liquid water absorbs in the shortwave infrared, the normalized difference infrared index (NDII), calculated from Landsat 5 Thematic Mapper band 4 (0.76-0.90 mu m wavelength) and band 5 (1.55-1.65 mu m wavelength), can be used to determine canopy equivalent water thickness (EWT), which is defined as the water volume per leaf area times the leaf area index (LAI). Alternatively, average canopy EWT can be determined using a landcover classification, because different vegetation types have different average LAI at the peak of the growing season. The primary contribution of this study for the Soil Moisture Experiment 2004 was to sample vegetation for the Axizona and Sonora study areas. Vegetation was sampled to achieve a range of canopy EWT; LAI was measured using a plant canopy analyzer and digital hemispherical (fisheye) photographs. NDII was linearly related to measured canopy EWT with an R-2 of 0.601. Landcover of the Arizona, USA, and Sonora, Mexico, study areas were classified with an overall accuracy of 70% using a rule-based decision tree using three dates of Landsat 5 Thematic Mapper imagery and digital elevation data. There was a large range of NDII per landcover class at the peak of the growing season, indicating that canopy EWT should be estimated directly using NDII or other shortwave-infrared vegetation indices. However, landcover classifications will still be necessary to obtain total vegetation water content from canopy EWT and other data, because considerable liquid water is contained in the non-foliar components of vegetation. Published by Elsevier Inc. C1 [Yilmaz, M. Tugrul; Hunt, E. Raymond, Jr.; Jackson, Thomas J.] USDA ARS, HRSL, Beltsville, MD 20705 USA. [Goins, Lyssa D.] Univ Arizona, Tucson, AZ USA. [Ustin, Susan L.] Univ Calif Davis, Dept Land Air & Water Resources, Davis, CA 95616 USA. [Vanderbilt, Vern C.] NASA, Ames Res Ctr, Moffett Field, CA USA. RP Hunt, ER (reprint author), USDA ARS, HRSL, Bldg 007,Room 104,BARC-W,10300 Baltimore Ave, Beltsville, MD 20705 USA. EM Raymond.Hunt@ars.usda.gov NR 53 TC 57 Z9 58 U1 0 U2 13 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 FEB 15 PY 2008 VL 112 IS 2 BP 350 EP 362 DI 10.1016/j.rse.2007.03.029 PG 13 WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic Technology SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science & Photographic Technology GA 261GW UT WOS:000253068100006 ER PT J AU Cheng, YB Ustin, SL Riano, D Vanderbilt, VC AF Cheng, Yen-Ben Ustin, Susan L. Riano, David Vanderbilt, Vem C. TI Water content estimation from hyperspectral images and MODIS indexes in Southeastern Arizona SO REMOTE SENSING OF ENVIRONMENT LA English DT Article DE AVIRIS; MODIS; water content; equivalent water thickness; vegetation index ID MODEL INVERSION METHODS; FUEL MOISTURE-CONTENT; BIOPHYSICAL PARAMETERS; VEGETATION INDEXES; MOJAVE-DESERT; WALNUT-GULCH; AVIRIS DATA; LEAF; REFLECTANCE; CANOPIES AB Hyperspectral water retrievals from AVIRIS data, equivalent water thickness (EWT), were compared to in situ leaf water content and LAI measurements at a semiarid site in southeastern Arizona. Retrievals of EWT showed good correlation with field canopy water content measurements. Statistical analysis suggested that EWT was significantly different among seven community types, from savanna to agriculture. Four band-ratio indexes (NDVI, EVI, NDWI, and NDII) were derived from MODIS showing strong spatial agreement between maps of AVIRIS EWT and MODIS indexes, and good statistical agreement for the range of habitats at the site. Temporal patterns of these four indexes in all vegetation communities except creosote bush and agriculture showed distinct seasonal patterns that responded to the timing and amount of precipitation. Moreover, these time series captured different ecological responses among the different vegetation communities. (C) 2007 Elsevier Inc. All rights reserved. C1 [Cheng, Yen-Ben; Ustin, Susan L.; Riano, David] Univ Calif Davis, CSTARS, Dept Land Air & Water Resources, Davis, CA 95616 USA. [Riano, David] Univ Alcala de Henares, Dept Geog, E-28801 Madrid, Spain. [Vanderbilt, Vem C.] NASA, Ames Res Ctr, Moffett Field, CA USA. RP Cheng, YB (reprint author), Univ Calif Davis, CSTARS, 1 Shields Ave, Davis, CA 95616 USA. EM ybcheng@cstars.ucdavis.edu RI Cheng, Yen-Ben/G-1311-2012; Riano, David/C-9663-2013 OI Riano, David/0000-0002-0198-1424 NR 54 TC 49 Z9 54 U1 3 U2 22 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 FEB 15 PY 2008 VL 112 IS 2 BP 363 EP 374 DI 10.1016/j.rse.2007.01.023 PG 12 WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic Technology SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science & Photographic Technology GA 261GW UT WOS:000253068100007 ER PT J AU Thoma, DP Moran, MS Bryant, R Rahman, MM Collins, CDH Keefer, TO Noriega, R Osman, I Skrivin, SM Tischler, MA Bosch, DD Starks, PJ Peters-Lidard, CD AF Thoma, D. P. Moran, M. S. Bryant, R. Rahman, M. M. Collins, C. D. Holifield Keefer, T. O. Noriega, R. Osman, I. Skrivin, S. M. Tischler, M. A. Bosch, D. D. Starks, P. J. Peters-Lidard, C. D. TI Appropriate scale of soil moisture retrieval from high resolution radar imagery for bare and minimally vegetated soils SO REMOTE SENSING OF ENVIRONMENT LA English DT Article DE radar; soil moisture; scale ID SAR DATA; SURFACE; BACKSCATTERING; NOISE; MODEL AB This research investigates the appropriate scale for watershed averaged and site specific soil moisture retrieval from high resolution radar imagery. The first approach involved filtering backscatter for input to a retrieval model that was compared against field measures of soil moisture. The second approach involved spatially averaging raw and filtered imagery in an image-based statistical technique to determine the best scale for site-specific soil moisture retrieval. Field soil moisture was measured at 1225 m(2) sites in three watersheds commensurate with 7 m resolution Radarsat image acquisition. Analysis of speckle reducing block median filters indicated that 5 x 5 filter level was the optimum for watershed averaged estimates of soil moisture. However, median filtering alone did not provide acceptable accuracy for soil moisture retrieval on a site-specific basis. Therefore, spatial averaging of unfiltered and median filtered power values was used to generate backscatter estimates with known confidence for soil moisture retrieval. This combined approach of filtering and averaging was demonstrated at watersheds located in Arizona (AZ), Oklahoma (OK) and Georgia (GA). The optimum ground resolution for AZ, OK and GA study areas was 162 m, 310 m, and 1131 m respectively obtained with unfiltered imagery. This statistical approach does not rely on ground verification of soil moisture for validation and only requires a satellite image and average roughness parameters of the site. When applied at other locations, the resulting optimum ground resolution will depend on the spatial distribution of land surface features that affect radar backscatter. This work offers insight into the accuracy of soil moisture retrieval, and an operational approach to determine the optimal spatial resolution for the required application accuracy. Published by Elsevier Inc. C1 [Thoma, D. P.; Moran, M. S.; Bryant, R.; Collins, C. D. Holifield; Keefer, T. O.; Skrivin, S. M.] USDA ARS, SW Watershed Res Ctr, Tucson, AZ 85719 USA. [Rahman, M. M.] Saskatchewan Environm Planning & Risk Analysis Di, Regina, SK, Canada. [Osman, I.] Univ Arizona, Tucson, AZ 85721 USA. [Tischler, M. A.] USA, Corps Eng Topog Engn Ctr, Alexandria, VA USA. [Bosch, D. D.] USDA ARS, SE Watershed Res Ctr, Tifton, GA 31793 USA. [Starks, P. J.] USDA ARS, Nat Resources Res Unit, El Reno, OK USA. [Peters-Lidard, C. D.] NASA, Goddard Space Flight Ctr, Hydrol Sci Branch Code 6143, Greenbelt, MD USA. RP Thoma, DP (reprint author), USDA ARS, SW Watershed Res Ctr, Tucson, AZ 85719 USA. EM dave_thoma@nps.gov RI Peters-Lidard, Christa/E-1429-2012 OI Peters-Lidard, Christa/0000-0003-1255-2876 NR 29 TC 29 Z9 30 U1 2 U2 11 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 FEB 15 PY 2008 VL 112 IS 2 BP 403 EP 414 DI 10.1016/j.rse.2007.06.021 PG 12 WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic Technology SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science & Photographic Technology GA 261GW UT WOS:000253068100010 ER PT J AU Schroeder, W Csiszar, I Morisette, J AF Schroeder, Wilfrid Csiszar, Ivan Morisette, Jeffrey TI Quantifying the impact of cloud obscuration on remote sensing of active fires in the Brazilian Amazon SO REMOTE SENSING OF ENVIRONMENT LA English DT Article DE vegetation fires; clouds; geostationary satelite; Brazilian amazon ID BOREAL FOREST REGION; SOUTH-AMERICA; DETECTION ALGORITHMS; RAINFALL ESTIMATION; TROPICAL FORESTS; VEGETATION FIRE; TRMM VIRS; SCAR-B; BIOMASS; EMISSIONS AB Vegetation fires remain as one of the most important processes governing land use and land cover change in tropical areas. The large area extent of fire prone areas associated with human activities makes satellite remote sensing of active fires a valuable tool to help monitor biomass burning in those regions. However, identification of active fire fronts under optically thick clouds is not possible through passive remote sensing, often resulting in omission errors. Previous analyses of fire activity either ignored the cloud obscuration problem or applied corrections based on the assumption that fire occurrence is not impacted by the presence of clouds. In this study we addressed the cloud obscuration problem in the Brazilian Amazon region using a pixel based probabilistic approach, using information on previous fire occurrence, precipitation and land use. We implemented the methodology using data from the geostationary GOES imager, covering the entire diurnal cycle of fire activity and cloud occurrence. Our assessment of the method indicated that the cloud adjustment reproduced the number of potential fires missed within 1.5% and 5% of the true fire counts on annual and monthly bases respectively. Spatially explicit comparison with high resolution burn scar maps in Acre state showed a reduction of omission error (from 58.3% to 43.7%) and only slight increase of commission error (from 6.4% to 8.8%) compared to uncorrected fire counts. A basin-wide analysis of corrected GOES fire counts during 2005 showed a mean cloud adjustment factor of approximately 11%, ranging from negligible adjustment in the central and western part of the Brazilian Amazon to as high as 50% in parts of Roraima, Para and Mato Grosso. (C) 2007 Elsevier Inc. All rights reserved. C1 [Schroeder, Wilfrid; Csiszar, Ivan] Univ Maryland, Dept Geog, College Pk, MD 20742 USA. [Morisette, Jeffrey] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Schroeder, W (reprint author), Univ Maryland, Dept Geog, 2181 LeFrak Hall, College Pk, MD 20742 USA. EM schroeder@hermes.geog.umd.edu RI Csiszar, Ivan/D-2396-2010; Schroeder, Wilfrid/F-6738-2010 NR 52 TC 29 Z9 29 U1 3 U2 17 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 FEB 15 PY 2008 VL 112 IS 2 BP 456 EP 470 DI 10.1016/j.rse.2007.05.004 PG 15 WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic Technology SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science & Photographic Technology GA 261GW UT WOS:000253068100014 ER PT J AU Tarnavsky, E Garrigues, S Brown, ME AF Tarnavsky, Elena Garrigues, Sebastien Brown, Molly E. TI Multiscale geostatistical analysis of AVHRR, SPOT-VGT, and MODIS global NDVI products SO REMOTE SENSING OF ENVIRONMENT LA English DT Article DE AVHRR; SPOT-VGT; MODIS; Landsat; NDVI; geostatistics; variograms; variogram modeling; spatial variability; variogram sill; length scale; EOS sites; global vegetation monitoring; multisensor; multiscale ID VEGETATION INDEXES; DIGITAL IMAGES; BIOPHYSICAL VARIABLES; AUTO-CORRELATION; VALIDATION; SURFACE; MODELS; REGULARIZATION; REFLECTANCE; VARIOGRAMS AB Global NDVI data are routinely derived from the AVHRR, SPOT-VGT, and MODIS/Terra earth observation records for a range of applications from terrestrial vegetation monitoring to climate change modeling. This has led to a substantial interest in the harmonization of multisensor records. Most evaluations of the internal consistency and continuity of global multisensor NDVI products have focused on time-series harmonization in the spectral domain, often neglecting the spatial domain. We fill this void by applying variogram modeling (a) to evaluate the differences in spatial variability between 8-km AVHRR, 1-km SPOT-VGT, and 1-km, 500-m, and 250-m MODIS NDVI products over eight EOS (Earth Observing System) validation sites, and (b) to characterize the decay of spatial variability as a function of pixel size (i.e. data regularization) for spatially aggregated Landsat ETM+ NDVI products and a real multisensor dataset. First, we demonstrate that the conjunctive analysis of two variogram properties - the sill and the mean length scale metric - provides a robust assessment of the differences in spatial variability between multiscale NDVI products that are due to spatial (nominal pixel size, point spread function, and view angle) and non-spatial (sensor calibration, cloud clearing, atmospheric corrections, and length of multi-day compositing period) factors. Next, we show that as the nominal pixel size increases, the decay of spatial information content follows a logarithmic relationship with stronger fit value for the spatially aggregated NDVI products (R-2 = 0.9321) than for the native resolution AVHRR, SPOT-VGT, and MODIS NDVI products (R-2 = 0.5064). This relationship serves as a reference for evaluation of the differences in spatial variability and length scales in multiscale datasets at native or aggregated spatial resolutions. The outcomes of this study suggest that multisensor NDVI records cannot be integrated into a long-term data record without proper consideration of all factors affecting their spatial consistency. Hence, we propose an approach for selecting the spatial resolution, at which differences in spatial variability between NDVI products from multiple sensors are minimized. This approach provides practical guidance for the harmonization of long-term multisensor datasets. (C) 2007 Elsevier Inc. All rights reserved. C1 [Tarnavsky, Elena] Kings Coll London, Dept Geog, London, England. [Garrigues, Sebastien] Univ Maryland, NASA, Goddard Space Flight Ctr, College Pk, MD 20742 USA. [Brown, Molly E.] NASA, Goddard Space Flight Ctr, Sci Syst & Applicat Inc, Washington, DC USA. RP Tarnavsky, E (reprint author), Kings Coll London, Dept Geog, London, England. EM elena.tarnavsky@kcl.ac.uk RI Brown, Molly/E-2724-2010; Brown, Molly/M-5146-2013; OI Brown, Molly/0000-0001-7384-3314; Brown, Molly/0000-0001-7384-3314; Tarnavsky, Elena/0000-0003-3403-0411 NR 57 TC 84 Z9 93 U1 5 U2 49 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 FEB 15 PY 2008 VL 112 IS 2 BP 535 EP 549 DI 10.1016/j.rse.2007.05.008 PG 15 WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic Technology SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science & Photographic Technology GA 261GW UT WOS:000253068100020 ER PT J AU Garrigues, S Allard, D Baret, F AF Garrigues, S. Allard, D. Baret, F. TI Modeling temporal changes in surface spatial heterogeneity over an agricultural site SO REMOTE SENSING OF ENVIRONMENT LA English DT Article DE spatial heterogeneity; spatio-temporal variogram model; NDVI; phenology; agricultural site; crop seasonal trajectory; spatial structure; landscape; high spatial resolution imagery; moderate spatial resolution imagery; non-linear estimation process; scaling bias ID REMOTE-SENSING ALGORITHMS; SATELLITE MEASUREMENTS; SOIL-MOISTURE; SCALE; DISAGGREGATION AB High temporal frequency remote sensing observations are required to monitor vegetation functioning. These observations are currently provided by moderate resolution sensor (with pixel size ranging from 250 m to 10 km). However, the intra-pixel spatial heterogeneity which may be important at moderate resolution, induces a scaling bias on non-linear estimation processes of land surface variable. A possible strategy to correct this scaling bias consists in using variogram model of high spatial resolution data (e.g. SPOT/HRV 20 m) as a proxy for the spatial heterogeneity within moderate resolution pixel. However, ways have to be found to get prior knowledge of this intra-pixel spatial heterogeneity metric without systematic concurrent high spatial resolution images. This paper aims at proposing a spatio-temporal model of the variogram of high spatial resolution data, which enables us to retrieve the spatial heterogeneity within moderate spatial resolution pixel using a temporal sampling of few high spatial resolution scenes. It capitalizes on variogram modeling of a time series of high spatial resolution NDVI images to quantify and model the temporal changes in landscape spatial heterogeneity over a particular crop site (Fundulea, Romania). We first demonstrate that important temporal variations in surface spatial heterogeneity observed over an agricultural site mainly result from the shift in seasonal trajectories between crop classes (here winter versus summer crops). The mean length scale as measured by the variogram integral range is mainly influenced by the gathering of fields with similar NDVI values. The scene overall spatial variability and the spatial heterogeneity within moderate resolution pixels, as quantified by the variogram. sill and the dispersion variance, respectively, increase with the difference in NDVI between winter and summer crops. The influence of surface spatial heterogeneity on the description of land surface processes is thus critical when the phenological variability between crop classes is maximum, suggesting that the number of high spatial resolution scenes should increase at these periods of the seasonal cycle. Then, based on these observations, we build a model describing the temporal course of surface spatial heterogeneity, i.e. the temporal trajectory of the variogram of high spatial resolution NDVI image, as a function of crop seasonality. Once calibrated from a temporal sampling of few high spatial resolution scenes, this model proves to be powerful to predict the variogram at a date at which the high spatial resolution scene is not available and thus to retrieve the spatial heterogeneity within moderate resolution pixels through the seasonal cycle within a mean relative uncertainty of 20%. (C) 2007 Elsevier Inc. All rights reserved. C1 [Garrigues, S.] Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20742 USA. [Allard, D.] INRA, Biostatist & Processus Spatiaux, Avignon, France. [Baret, F.] INRA, UMR1114, Avignon, France. RP Garrigues, S (reprint author), NASA, Goddard Space Flight Ctr, Mail Code 614 4, Greenbelt, MD 20771 USA. EM Sebastien.garrigues@gsfc.nasa.gov RI Baret, Fred/C-4135-2011 OI Baret, Fred/0000-0002-7655-8997 NR 30 TC 11 Z9 14 U1 5 U2 35 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 FEB 15 PY 2008 VL 112 IS 2 BP 588 EP 602 DI 10.1016/j.rse.2007.05.014 PG 15 WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic Technology SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science & Photographic Technology GA 261GW UT WOS:000253068100024 ER PT J AU Dong, XQ Minnis, P Xi, B Sun-, S Chen, Y AF Dong, Xiquan Minnis, Patrick Xi, Baike Sun-Mack, Sunny Chen, Yan TI Comparison of CERES-MODIS stratus cloud properties with ground-based measurements at the DOE ARM southern great plains site SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID ENERGY SYSTEM CERES; RADIATIVE PROPERTIES; INFRARED RADIANCES; SOLAR-RADIATION; SATELLITE; SURFACE; CLIMATE; RADAR; FIRE; PARAMETERIZATIONS AB Overcast stratus cloud properties derived for the Clouds and the Earth's Radiant Energy System (CERES) project using Terra and Aqua Moderate Resolution Imaging Spectroradiometer (MODIS) data are compared with observations taken at the Department of Energy (DOE) Atmospheric Radiation Measurement (ARM) Southern Great Plains site from March 2000 through December 2004. Retrievals from ARM surface-based data were averaged over a 1-h interval centered at the time of each satellite overpass, and the CERES-MODIS cloud properties were averaged within a 30 km x 30 km box centered on the ARM SGP site. Two data sets were analyzed: all of the data (ALL), which include multilayered, single-layered, and slightly broken stratus decks and a subset, single-layered unbroken decks (SL). The CERES-MODIS effective cloud heights were determined from effective cloud temperature using a lapse rate method with the surface temperature specified as the 24-h mean surface air temperature. For SL stratus, they are, on average, within the ARM radar-lidar estimated cloud boundaries and are 0.534 +/- 0.542 km and 0.108 +/- 0.480 km lower than the cloud physical tops and centers, respectively, and are comparable for day and night observations. The mean differences and standard deviations are slightly larger for ALL data, but not statistically different to those of SL data. The MODIS-derived effective cloud temperatures are 2.7 +/- 2.4 K less than the surface-observed SL cloud center temperatures with very high correlations (0.86-0.97). Variations in the height differences are mainly caused by uncertainties in the surface air temperatures, lapse rates, and cloud top height variability. The biases are mainly the result of the differences between effective and physical cloud top, which are governed by cloud liquid water content and viewing zenith angle, and the selected lapse rate, -7.1 K km(-1). On the basis of a total of 43 samples, the means and standard deviations of the differences between the daytime Terra and surface retrievals of effective radius re, optical depth, and liquid water path for SL stratus are 0.1 +/- 1.9 mu m (1.2 +/- 23.5%), -1.3 +/- 9.5 (-3.6 +/- 26.2%), and 0.6 +/- 49.9 gm(-2) (0.3 +/- 27%), respectively, while the corresponding correlation coefficients are 0.44, 0.87, and 0.89. For Aqua, they are 0.2 +/- 1.9 mm (2.5 +/- 23.4%), 2.5 +/- 7.8 (7.8 +/- 24.3%), and 28.1 +/- 52.7 gm(-2) (17.2 +/- 32.2%), as well as 0.35, 0.96, and 0.93 from a total of 21 cases. The results for ALL cases are comparable. Although a bias in r(e) was expected because the satellite retrieval of effective radius only represents the top of the cloud, the surface-based radar retrievals revealed that the vertical profile of r(e) is highly variable with smaller droplets occurring at cloud top in some cases. The larger bias in optical depth and liquid water path for Aqua is due, at least partially, to differences in the Terra and Aqua MODIS visible channel calibrations. Methods for improving the cloud top height and microphysical property retrievals are suggested. C1 [Dong, Xiquan; Xi, Baike] Univ N Dakota, Dept Atmospher Sci, Grand Forks, ND 58202 USA. [Sun-Mack, Sunny; Chen, Yan] Sci Applicat Int Corp Inc, Hampton, VA 23666 USA. [Minnis, Patrick] NASA, Langley Res Ctr, Hampton, VA 23681 USA. RP Dong, XQ (reprint author), Univ N Dakota, Dept Atmospher Sci, 4149 Univ Dr,Stop 9006, Grand Forks, ND 58202 USA. EM dong@aero.und.edu RI Minnis, Patrick/G-1902-2010; OI Minnis, Patrick/0000-0002-4733-6148; Dong, Xiquan/0000-0002-3359-6117 NR 48 TC 46 Z9 49 U1 1 U2 7 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X EI 2169-8996 J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD FEB 14 PY 2008 VL 113 IS D3 AR D03204 DI 10.1029/2007JD008438 PG 17 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 263RH UT WOS:000253233700001 ER PT J AU Schwarz, JP Spackman, JR Fahey, DW Gao, RS Lohmann, U Stier, P Watts, LA Thomson, DS Lack, DA Pfister, L Mahoney, MJ Baumgardner, D Wilson, JC Reeves, JM AF Schwarz, J. P. Spackman, J. R. Fahey, D. W. Gao, R. S. Lohmann, U. Stier, P. Watts, L. A. Thomson, D. S. Lack, D. A. Pfister, L. Mahoney, M. J. Baumgardner, D. Wilson, J. C. Reeves, J. M. TI Coatings and their enhancement of black carbon light absorption in the tropical atmosphere SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID OPTICAL-PROPERTIES; CLIMATE RESPONSE; SOOT PARTICLES; AEROSOL; CLOUDS; SCATTERING; TEMPERATURE; ALBEDO AB Black carbon ( BC) is the dominant aerosol absorber of solar radiation in the atmosphere and is an important component of anthropogenic climate forcing. BC's role is strongly dependent on its physical state, which can influence the way that BC particles may act as ice and cloud nuclei, as well as the way they interact with solar radiation. In situ measurements made with a single-particle soot photometer flown on a NASA high-altitude research aircraft show the mass and size of individual BC particles in the tropics, as well as their propensity to be found mixed with additional materials. Mie theory was used to connect observed light scattering off BC particles to the optical effects of coatings on the particles. The observations indicate that as BC from ground-based emission sources rises in altitude to the lower stratosphere, coatings on BC particles become both thicker and more prevalent, while BC mass mixing ratios decrease dramatically from their values near the ground. Coatings enhance light absorption by the ambient BC column by at least 30%. These results reveal the microphysical state of BC in the atmosphere while providing important constraints for models evaluating BC's role in climate change. C1 [Schwarz, J. P.; Spackman, J. R.; Fahey, D. W.; Gao, R. S.; Watts, L. A.; Thomson, D. S.; Lack, D. A.] NOAA, Div Chem Sci, Earth Syst Res Lab, Boulder, CO 80305 USA. [Baumgardner, D.] Univ Nacl Autonoma Mexico, Ctr Ciencias Atmosfera, Mexico City 04510, DF, Mexico. [Lohmann, U.] ETH, Inst Atmosphar & Klima, CH-8092 Zurich, Switzerland. [Mahoney, M. J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Pfister, L.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Wilson, J. C.; Reeves, J. M.] Univ Denver, Dept Engn, Denver, CO 80208 USA. [Stier, P.] CALTECH, Dept Environm Sci & Engn, Pasadena, CA 91125 USA. RP Schwarz, JP (reprint author), NOAA, Div Chem Sci, Earth Syst Res Lab, Boulder, CO 80305 USA. EM joshua.p.schwarz@noaa.gov RI Gao, Ru-Shan/H-7455-2013; Watts, Laurel/G-4532-2013; Fahey, David/G-4499-2013; Lohmann, Ulrike/B-6153-2009; Manager, CSD Publications/B-2789-2015; Stier, Philip/B-2258-2008; Lack, Daniel/I-9053-2012; schwarz, joshua/G-4556-2013 OI Watts, Laurel/0000-0002-0834-3329; Fahey, David/0000-0003-1720-0634; Lohmann, Ulrike/0000-0001-8885-3785; Stier, Philip/0000-0002-1191-0128; schwarz, joshua/0000-0002-9123-2223 NR 40 TC 123 Z9 126 U1 16 U2 69 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 FEB 14 PY 2008 VL 113 IS D3 AR D03203 DI 10.1029/2007JD009042 PG 10 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 263RH UT WOS:000253233700002 ER PT J AU Liu, X Shemansky, DE Malone, CP Johnson, PV Ajello, JM Kanik, I Heays, AN Lewis, BR Gibson, ST Stark, G AF Liu, Xianming Shemansky, Donald E. Malone, Charles P. Johnson, Paul V. Ajello, Joseph M. Kanik, Isik Heays, Alan N. Lewis, Brenton R. Gibson, Stephen T. Stark, Glenn TI Experimental and coupled-channels investigation of the radiative properties of the N(2)c(4)'(1)Sigma(+)(u)-X-1 Sigma(+)(g) band system SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article ID ELECTRON-IMPACT EXCITATION; HIGH-RESOLUTION ABSORPTION; ULTRAVIOLET EMISSION-SPECTRUM; SINGLET UNGERADE STATES; MOLECULAR NITROGEN; OSCILLATOR-STRENGTHS; RYDBERG STATES; CROSS-SECTION; LIFETIME MEASUREMENTS; LASER SPECTROSCOPY AB The emission properties of the N-2 c(4)' (1)Sigma(+)(u) - X (1)Sigma(+)(g) band system have been investigated in a joint experimental and coupled-channels theoretical study. Relative intensities of the c(4)' (1)Sigma(+)(u)(0) - X (1)Sigma(+()(g)v(i)) transitions, measured via electron-impact-induced emission spectroscopy, are combined with a coupled-channel Schrodinger equation (CSE) model of the N-2 molecule, enabling determination of the diabatic electronic transition moment for the c(4)' (1)Sigma(+)(u) - X (1)Sigma(+)(g) system as a function of internuclear distance. The CSE rotational transition probabilities are further verified by comparison with a high-resolution experimental spectrum. Spontaneous transition probabilities of the c(4)' (1)Sigma(+)(u) - X (1)Sigma(+)(g) band system, required for modeling atmospheric emission, can now be calculated reliably. C1 [Liu, Xianming; Shemansky, Donald E.] Space Environm Technol, Planetary & Space Sci Div, Pasadena, CA 91107 USA. [Malone, Charles P.; Johnson, Paul V.; Ajello, Joseph M.; Kanik, Isik] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Heays, Alan N.; Lewis, Brenton R.; Gibson, Stephen T.] Australian Natl Univ, Res Sch Phys Sci & Engn, Canberra, ACT 0200, Australia. [Stark, Glenn] Wellesley Coll, Dept Phys, Wellesley, MA 02181 USA. RP Liu, X (reprint author), Space Environm Technol, Planetary & Space Sci Div, 320 N Halstead, Pasadena, CA 91107 USA. EM xliu@spacenvironment.net; dshemansky@spacenvironment.net; charles.malone@jpl.nasa.gov; paul.v.johnson@jpl.nasa.gov; alan.heays@anu.edu.au; brenton.lewis@anu.edu.au; gstark@wellesley.edu RI Malone, Charles/A-6294-2010; Johnson, Paul/D-4001-2009 OI Malone, Charles/0000-0001-8418-1539; Johnson, Paul/0000-0002-0186-8456 NR 84 TC 18 Z9 18 U1 0 U2 8 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0148-0227 J9 J GEOPHYS RES-SPACE JI J. Geophys. Res-Space Phys. PD FEB 14 PY 2008 VL 113 IS A2 AR A02304 DI 10.1029/2007JA012787 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 263SM UT WOS:000253236800001 ER PT J AU Lyatsky, W Khazanov, GV AF Lyatsky, Wladislaw Khazanov, George V. TI Effect of solar wind density on relativistic electrons at geosynchronous orbit SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID RADIATION BELT; GEOMAGNETIC STORMS; ACCELERATION; MAGNETOSPHERE; TIMESCALE AB We examined the relationship between relativistic (> 2 MeV) electron fluxes at geostationary orbit and two solar wind parameters, the speed and density. For the analysis, we used data of relativistic electron fluxes measured with GOES-8 spacecraft for 1997 - 2002 and GOES-10 spacecraft for 2003 - 2006, and solar wind data, provided by Goddard Space Flight Center. Using the correlation analysis, we found that not only solar wind speed but also solar wind density provides a strong effect on relativistic electrons: the relativistic electron fluxes increase with increasing solar wind speed and decrease with increasing solar wind density. In contrast to solar wind speed that shows the best correlation with electron fluxes after about two days only, the solar wind density shows the best correlation with the electron fluxes after about 15 hours. To separate the effects of solar wind speed and density, we examined events when solar wind speed varied insignificantly; in these events, the effect of solar wind density on the relativistic electrons remained strong. We found that the solar wind density, which may affect the loss of relativistic electrons, effectively controls the magnitude of relativistic electron fluxes at geostationary orbit, so that the strongest fluxes occurred almost exclusively during low-density solar wind conditions. Thus, our study showed that solar wind density is an important parameter that may significantly affect the loss of relativistic electrons and, as a result, the resulting magnitude of the electron fluxes at geostationary orbit. Citation: Lyatsky, W., and G. V. Khazanov ( 2008), Effect of solar wind density on relativistic electrons at geosynchronous orbit. C1 [Lyatsky, Wladislaw; Khazanov, George V.] NASA Marshall Space Flight Ctr, Huntsville, AL 35805 USA. RP Lyatsky, W (reprint author), NASA Marshall Space Flight Ctr, 320 Sparkman Dr, Huntsville, AL 35805 USA. EM lyatsky@cspar.uah.edu NR 21 TC 26 Z9 26 U1 0 U2 1 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 FEB 13 PY 2008 VL 35 IS 3 AR L03109 DI 10.1029/2007GL032524 PG 5 WC Geosciences, Multidisciplinary SC Geology GA 263QM UT WOS:000253231600005 ER PT J AU Maksym, T Markus, T AF Maksym, Ted Markus, Thorsten TI Antarctic sea ice thickness and snow-to-ice conversion from atmospheric reanalysis and passive microwave snow depth SO JOURNAL OF GEOPHYSICAL RESEARCH-OCEANS LA English DT Article ID OPERATIONAL NUMERICAL-ANALYSES; SURFACE MASS-BALANCE; WESTERN WEDDELL-SEA; SOUTHERN-OCEAN; TEMPORAL VARIABILITY; PACK ICE; BELLINGSHAUSEN SEAS; AMUNDSEN SEAS; LATE WINTER; ROSS SEA AB Passive microwave snow depth, ice concentration, and ice motion estimates are combined with snowfall from the European Centre for Medium-Range Weather Forecasting (ECMWF) reanalysis (ERA-40) from 1979-2001 to estimate the prevalence of snow-to-ice conversion (snow-ice formation) on level sea ice in the Antarctic for April-October. Snow ice is ubiquitous in all regions throughout the growth season. Calculated snow-ice thicknesses fall within the range of estimates from ice core analysis for most regions. However, uncertainties in both this analysis and in situ data limit the usefulness of snow depth and snow-ice production to evaluate the accuracy of ERA-40 snowfall. The East Antarctic is an exception, where calculated snow-ice production exceeds observed ice thickness over wide areas, suggesting that ERA-40 precipitation is too high there. Snow-ice thickness variability is strongly controlled not just by snow accumulation rates, but also by ice divergence. Surprisingly, snow-ice production is largely independent of snow depth, indicating that the latter may be a poor indicator of total snow accumulation. Using the presence of snow-ice formation as a proxy indicator for near-zero freeboard, we examine the possibility of estimating level ice thickness from satellite snow depths. A best estimate for the mean level ice thickness in September is 53 cm, comparing well with 51 cm from ship-based observations. The error is estimated to be 10-20 cm, which is similar to the observed interannual and regional variability. Nevertheless, this is comparable to expected errors for ice thickness determined by satellite altimeters. Improvement in satellite snow depth retrievals would benefit both of these methods. C1 [Maksym, Ted] British Antarctic Survey, Cambridge CB3 0ET, England. [Markus, Thorsten] NASA Goddard Space Flight Ctr, Greenbelt, MD USA. RP Maksym, T (reprint author), British Antarctic Survey, Cambridge CB3 0ET, England. RI Markus, Thorsten/D-5365-2012 NR 85 TC 30 Z9 31 U1 0 U2 5 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0148-0227 J9 J GEOPHYS RES-OCEANS JI J. Geophys. Res.-Oceans PD FEB 13 PY 2008 VL 113 IS C2 AR C02S12 DI 10.1029/2006JC004085 PG 18 WC Oceanography SC Oceanography GA 263RZ UT WOS:000253235500003 ER PT J AU Dlugach, JM Mishchenko, MI AF Dlugach, Janna M. Mishchenko, Michael I. TI Photopolarimetry of planetary atmospheres: what observational data are essential for a unique retrieval of aerosol microphysics? SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE polarization; scattering; techniques : photometric; techniques : polarimetric; planets and satellites : individual : Jupiter ID ELECTROMAGNETIC SCATTERING; LIGHT-SCATTERING; RADIATIVE PROPERTIES; OPTICAL-PROPERTIES; JOVIAN ATMOSPHERE; POLARIZED-LIGHT; JUPITER; PARTICLES; CLOUDS; VENUS AB We analyse the results of computations of the intensity and degree of linear polarization of diffusely reflected sunlight for the centre of a planetary disc in the phase-angle range 0 degrees = 12 degrees. Thus, using Jupiter as a 'proving ground', we conclude that only polatimetric data obtained over a wide range of phase angles (i.e. from spacecraft) may provide definitive constraints on aerosol shape and, as a consequence, ameliorate the ill-posed nature of the inverse remote-sensing problem. C1 [Mishchenko, Michael I.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA. [Dlugach, Janna M.] Natl Acad Sci Ukraine, Main Astron Observ, UA-03680 Kiev, Ukraine. RP Mishchenko, MI (reprint author), NASA, Goddard Inst Space Studies, 2880 Broadwy, New York, NY 10025 USA. EM mmishchenko@giss.nasa.gov RI Mishchenko, Michael/D-4426-2012 NR 37 TC 6 Z9 6 U1 0 U2 6 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 FEB 11 PY 2008 VL 384 IS 1 BP 64 EP 70 DI 10.1111/j.1365-2966.2007.12679.x PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 264TC UT WOS:000253312300004 ER PT J AU Ade, P Bock, J Bowden, M Brown, ML Cahill, G Carlstrom, JE Castro, PG Church, S Culverhouse, T Friedman, R Ganga, K Gear, WK Hinderks, J Kovac, J Lange, AE Leitch, E Melhuish, SJ Murphy, JA Orlando, A Schwarz, R O'Sullivan, C Piccirillo, L Pryke, C Rajguru, N Rusholme, B Taylor, AN Thompson, KL Wu, EYS Zemcov, M AF Ade, P. Bock, J. Bowden, M. Brown, M. L. Cahill, G. Carlstrom, J. E. Castro, P. G. Church, S. Culverhouse, T. Friedman, R. Ganga, K. Gear, W. K. Hinderks, J. Kovac, J. Lange, A. E. Leitch, E. Melhuish, S. J. Murphy, J. A. Orlando, A. Schwarz, R. O'Sullivan, C. Piccirillo, L. Pryke, C. Rajguru, N. Rusholme, B. Taylor, A. N. Thompson, K. L. Wu, E. Y. S. Zemcov, M. TI First season QUaD CMB temperature and polarization power spectra SO ASTROPHYSICAL JOURNAL LA English DT Article DE polarization ID PROBE WMAP OBSERVATIONS; COSMIC BACKGROUND IMAGER; 2003 FLIGHT; MICROWAVE; ANISOTROPY; BOOMERANG AB QUaD is a bolometric CMB polarimeter sited at the South Pole, operating at frequencies of 100 and 150 GHz. In this paper we report preliminary results from the first season of operation ( austral winter 2005). All six CMB power spectra are presented derived as cross spectra between the 100 and 150 GHz maps using 67 days of observation in a low foreground region of approximately 60 deg(2). These data are a small fraction of the data acquired to date. The measured spectra are consistent with the Lambda CDM cosmological model. We perform jackknife tests that indicate that the observed signal has negligible contamination from instrumental systematics. In addition, by using a frequency jackknife we find no evidence for foreground contamination. C1 [Ade, P.; Bowden, M.; Gear, W. K.; Melhuish, S. J.; Orlando, A.; Piccirillo, L.; Rajguru, N.; Zemcov, M.] Cardiff Univ, Sch Phys & Astron, Cardiff CF24 3AA, S Glam, Wales. [Bock, J.; Leitch, E.; Zemcov, M.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Bock, J.; Kovac, J.; Lange, A. E.; Zemcov, M.] CALTECH, Pasadena, CA 91125 USA. [Bowden, M.; Hinderks, J.; Rusholme, B.; Thompson, K. L.; Wu, E. Y. S.] Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, Stanford, CA 94305 USA. [Brown, M. L.; Castro, P. G.; Taylor, A. N.] Univ Edinburgh, Royal Observ, Inst Astron, Edinburgh EH9 3HJ, Midlothian, Scotland. [Cahill, G.; Murphy, J. A.; O'Sullivan, C.] Natl Univ Ireland Maynooth, Dept Expt Phys, Maynooth, Kildare, Ireland. [Carlstrom, J. E.; Culverhouse, T.; Friedman, R.; Schwarz, R.; Pryke, C.] Univ Chicago, Dept Astron & Astrophys, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA. [Ganga, K.] CNRS, Lab APC, F-75205 Paris 13, France. [Rajguru, N.] UCL, Dept Phys & Astron, London WC1E 6BT, England. RP Ade, P (reprint author), Cardiff Univ, Sch Phys & Astron, Queens Bldg, Cardiff CF24 3AA, S Glam, Wales. RI Melhuish, Simon/B-1299-2016; OI Melhuish, Simon/0000-0001-8725-4991; Orlando, Angiola/0000-0001-8004-5054 NR 24 TC 57 Z9 57 U1 0 U2 1 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 FEB 10 PY 2008 VL 674 IS 1 BP 22 EP 28 DI 10.1086/524922 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 266RJ UT WOS:000253454400003 ER PT J AU Kuntz, KD Snowden, SL AF Kuntz, K. D. Snowden, S. L. TI The X-ray-emitting components toward l=111 degrees: The local hot bubble and beyond SO ASTROPHYSICAL JOURNAL LA English DT Article DE X-rays : diffuse background ID XMM-NEWTON OBSERVATION; INTERSTELLAR-MEDIUM; MOLECULAR CLOUDS; CHANDRA OBSERVATIONS; CO SURVEY; EMISSION; SOLAR; GAS; ABSORPTION; GALAXIES AB We have obtained an XMM-Newton spectrum of the diffuse X-ray emission toward (l, b) (111.14 degrees, 1.11 degrees), a line of sight with a relatively simple distribution of absorbing clouds: > 9 x 10(19) cm(-2) at R > 170 pc, a 6 x 10(21) cm(-2) molecular cloud at 2.5-3.3 kpc, and a total column of 1.2 x 10(22) cm(-2). We find that the analysis of the XMM-Newton spectrum in conjunction with the ROSAT All-Sky Survey (RASS) spectral energy distribution for the same direction requires three thermal components to be well fit: a "standard'' Local Hot Bubble component with kT = 0.095, a component beyond the molecular cloud with kT = 0.57, and a component before the molecular cloud with kT = 0.24. The strength of the O VII 0.56 keV line from the Local Hot Bubble, 1.75 +/- 0.7 photons cm(-2) s(-1) sr(-1), is consistent with other recent measures. The 0.24 keV component has an emission measure of 0.0021 +/- 0.0006 cm(-6) pc and is not localized save as diffuse emission within the Galactic plane. Rough calculations show that only about a quarter of this component is due to unresolved stellar emission; it is the best candidate for a pervasive hot medium. The spatial separation of the similar to 0.2 keV component from the similar to 0.6 keV component suggests that the spectral decompositions of the emission from late-type spiral disks found in the literature do represent real temperature components rather than reflecting more complex temperature distributions. C1 [Kuntz, K. D.; Snowden, S. L.] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA. [Kuntz, K. D.] Johns Hopkins Univ, Henry A Rowland Dept Phys & Astron, Baltimore, MD 21218 USA. RP Kuntz, KD (reprint author), NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Code 662, Greenbelt, MD 20771 USA. RI Snowden, Steven/D-5292-2012 NR 52 TC 14 Z9 14 U1 0 U2 1 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 FEB 10 PY 2008 VL 674 IS 1 BP 209 EP 219 DI 10.1086/524719 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 266RJ UT WOS:000253454400018 ER PT J AU Achterberg, A Ackermann, M Adams, J Ahrens, J Andeen, K Auffenberg, J Bahcall, JN Bai, X Baret, B Barwick, SW Bay, R Beattie, K Becka, T Becker, JK Becker, KH Berghaus, P Berley, D Bernardini, E Bertrand, D Besson, DZ Blaufuss, E Boersma, DJ Bohm, C Bolmont, J Boser, S Botner, O Bouchta, A Braun, J Burgess, C Burgess, T Castermans, T Chirkin, D Christy, B Clem, J Cowen, DF D'Agostino, MV Davour, A Day, CT De Clercq, C Demirores, L Descamps, F Desiati, P DeYoung, T Diaz-Velez, JC Dreyer, J Dumm, JP Duvoort, MR Edwards, WR Ehrlich, R Eisch, J Ellsworth, RW Evenson, PA Fadiran, O Fazely, AR Filimonov, K Foerster, MM Fox, BD Franckowiak, A Gaisser, TK Gallagher, J Ganugapati, R Geenen, H Gerhardt, L Goldschmidt, A Goodman, JA Gozzini, R Griesel, T Gross, A Grullon, S Gunasingha, RM Gurtner, M Hallgren, A Halzen, F Han, K Hanson, K Hardtke, D Hardtke, R Hart, JE Hasegawa, Y Hauschildt, T Hays, D Heise, J Helbing, K Hellwig, M Herquet, P Hill, GC Hodges, J Hoffman, KD Hommez, B Hoshina, K Hubert, D Hughey, B Hulth, PO Huss, JP Hultqvist, K Hundertmark, S Inaba, M Ishihara, A Jacobsen, J Japaridze, GS Johansson, H Jones, A Joseph, JM Kampert, KH Kappes, A Karg, T Karle, A Kawai, H Kelley, JL Kitamura, N Klein, SR Klepser, S Kohnen, G Kolanoski, H Pke, LK Kowalski, M Kowarik, T Krasberg, M Kuehn, K Labare, M Landsman, H Leich, H Leier, D Liubarsky, I Lundberg, J Lunemann, J Madsen, J Mase, K Matis, HS McCauley, T McParland, CP Meli, A Messarius, T Meszaros, P Miyamoto, H Mokhtarani, A Montaruli, T Morey, A Morse, R Movit, SM Munich, K Nahnhauer, R Nam, JW Niessen, P Nygren, DR Ogelman, H Olivas, A Patton, S Pena-Garay, C Heros, CPL Piegsa, A Pieloth, D Pohl, AC Porrata, R Pretz, J Price, PB Przybylski, GT Rawlins, K Razzaque, S Resconi, E Rhode, W Ribordy, M Rizzo, A Robbins, S Roth, P Rott, C Rutledge, D Ryckbosch, D Sander, HG Sarkar, S Schlenstedt, S Schmidt, T Schneider, D Seckel, D Semburg, B Seo, SH Seunarine, S Silvestri, A Smith, AJ Solarz, M Song, C Sopher, JE Spiczak, GM Spiering, C Stamatikos, M Stanev, T Steffen, P Stezelberger, T Stokstad, RG Stoufer, MC Stoyanov, S Strahler, EA Straszheim, T Sulanke, KH Sullivan, GW Sumner, TJ Taboada, I Tarasova, O Tepe, A Thollander, L Tilav, S Tluczykont, M Toale, PA Turcan, D Van Eijndhoven, N Vandenbroucke, J Van Overloop, A Viscomi, V Voigt, B Wagner, W Walck, C Waldmann, H Walter, M Wang, YR Wendt, C Wiebusch, CH Wikstrom, G Williams, DR Wischnewski, R Wissing, H Woschnagg, K Xu, XW Yodh, G Yoshida, S Zornoza, JD Boer, M Cline, T Crew, G Feroci, M Frontera, F Hurley, K Lamb, D Rau, A Rossi, F Ricker, G Von Kienlin, A AF Achterberg, A. Ackermann, M. Adams, J. Ahrens, J. Andeen, K. Auffenberg, J. Bahcall, J. N. Bai, X. Baret, B. Barwick, S. W. Bay, R. Beattie, K. Becka, T. Becker, J. K. Becker, K. -H. Berghaus, P. Berley, D. Bernardini, E. Bertrand, D. Besson, D. Z. Blaufuss, E. Boersma, D. J. Bohm, C. Bolmont, J. Boeser, S. Botner, O. Bouchta, A. Braun, J. Burgess, C. Burgess, T. Castermans, T. Chirkin, D. Christy, B. Clem, J. Cowen, D. F. D'Agostino, M. V. Davour, A. Day, C. T. De Clercq, C. Demiroeres, L. Descamps, F. Desiati, P. DeYoung, T. Diaz-Velez, J. C. Dreyer, J. Dumm, J. P. Duvoort, M. R. Edwards, W. R. Ehrlich, R. Eisch, J. Ellsworth, R. W. Evenson, P. A. Fadiran, O. Fazely, A. R. Filimonov, K. Foerster, M. M. Fox, B. D. Franckowiak, A. Gaisser, T. K. Gallagher, J. Ganugapati, R. Geenen, H. Gerhardt, L. Goldschmidt, A. Goodman, J. A. Gozzini, R. Griesel, T. Gross, A. Grullon, S. Gunasingha, R. M. Gurtner, M. Hallgren, A. Halzen, F. Han, K. Hanson, K. Hardtke, D. Hardtke, R. Hart, J. E. Hasegawa, Y. Hauschildt, T. Hays, D. Heise, J. Helbing, K. Hellwig, M. Herquet, P. Hill, G. C. Hodges, J. Hoffman, K. D. Hommez, B. Hoshina, K. Hubert, D. Hughey, B. Hulth, P. O. Huess, J. -P. Hultqvist, K. Hundertmark, S. Inaba, M. Ishihara, A. Jacobsen, J. Japaridze, G. S. Johansson, H. Jones, A. Joseph, J. M. Kampert, K. -H. Kappes, A. Karg, T. Karle, A. Kawai, H. Kelley, J. L. Kitamura, N. Klein, S. R. Klepser, S. Kohnen, G. Kolanoski, H. Pke, L. Ko Kowalski, M. Kowarik, T. Krasberg, M. Kuehn, K. Labare, M. Landsman, H. Leich, H. Leier, D. Liubarsky, I. Lundberg, J. Luenemann, J. Madsen, J. Mase, K. Matis, H. S. McCauley, T. McParland, C. P. Meli, A. Messarius, T. Meszaros, P. Miyamoto, H. Mokhtarani, A. Montaruli, T. Morey, A. Morse, R. Movit, S. M. Muenich, K. Nahnhauer, R. Nam, J. W. Niessen, P. Nygren, D. R. Oegelman, H. Olivas, A. Patton, S. Pena-Garay, C. De Los Heros, C. Perez Piegsa, A. Pieloth, D. Pohl, A. C. Porrata, R. Pretz, J. Price, P. B. Przybylski, G. T. Rawlins, K. Razzaque, S. Resconi, E. Rhode, W. Ribordy, M. Rizzo, A. Robbins, S. Roth, P. Rott, C. Rutledge, D. Ryckbosch, D. Sander, H. -G. Sarkar, S. Schlenstedt, S. Schmidt, T. Schneider, D. Seckel, D. Semburg, B. Seo, S. H. Seunarine, S. Silvestri, A. Smith, A. J. Solarz, M. Song, C. Sopher, J. E. Spiczak, G. M. Spiering, C. Stamatikos, M. Stanev, T. Steffen, P. Stezelberger, T. Stokstad, R. G. Stoufer, M. C. Stoyanov, S. Strahler, E. A. Straszheim, T. Sulanke, K. -H. Sullivan, G. W. Sumner, T. J. Taboada, I. Tarasova, O. Tepe, A. Thollander, L. Tilav, S. Tluczykont, M. Toale, P. A. Turcan, D. Van Eijndhoven, N. Vandenbroucke, J. Van Overloop, A. Viscomi, V. Voigt, B. Wagner, W. Walck, C. Waldmann, H. Walter, M. Wang, Y. -R. Wendt, C. Wiebusch, C. H. Wikstroem, G. Williams, D. R. Wischnewski, R. Wissing, H. Woschnagg, K. Xu, X. W. Yodh, G. Yoshida, S. Zornoza, J. D. Boer, M. Cline, T. Crew, G. Feroci, M. Frontera, F. Hurley, K. Lamb, D. Rau, A. Rossi, F. Ricker, G. Von Kienlin, A. TI The search for muon neutrinos from northern hemisphere gamma-ray bursts with amanda SO ASTROPHYSICAL JOURNAL LA English DT Article DE gamma rays : bursts; neutrinos ID HIGH-ENERGY NEUTRINOS; SUPERNOVAE; CONNECTION; TELESCOPES; DETECTORS; SELECTION; EMISSION; PARADIGM; BATSE; IB/C AB We present the results of the analysis of neutrino observations by the Antarctic Muon and Neutrino Detector Array (AMANDA) correlated with photon observations of more than 400 gamma-ray bursts (GRBs) in the northern hemisphere from 1997 to 2003. During this time period, AMANDA's effective collection area for muon neutrinos was larger than that of any other existing detector. After the application of various selection criteria to our data, we expect similar to 1 neutrino event and <2 background events. Based on our observations of zero events during and immediately prior to the GRBs in the data set, we set the most stringent upper limit on muon neutrino emission correlated with GRBs. Assuming a Waxman-Bahcall spectrum and incorporating all systematic uncertainties, our flux upper limit has a normalization at 1 PeV of E-2 Phi(nu) <= 6.3 x 10(-9) GeV cm(-2) s(-1) sr(-1), with 90% of the events expected within the energy range of similar to 10 TeV to similar to 3 PeV. The impact of this limit on several theoretical models of GRBs is discussed, as well as the future potential for detection of GRBs by next-generation neutrino telescopes. Finally, we briefly describe several modifications to this analysis in order to apply it to other types of transient point sources. C1 [Achterberg, A.; Duvoort, M. R.; Heise, J.; Van Eijndhoven, N.] Univ Utrecht, Dept Phys & Astron, NL-3584 CC Utrecht, Netherlands. [Ackermann, M.; Bernardini, E.; Bolmont, J.; Boeser, S.; Klepser, S.; Leich, H.; Nahnhauer, R.; Pieloth, D.; Schlenstedt, S.; Steffen, P.; Sulanke, K. -H.; Tarasova, O.; Tluczykont, M.; Voigt, B.; Waldmann, H.; Walter, M.; Wischnewski, R.] Deutsches Elektron Synchrotron, D-15735 Zeuthen, Germany. [Adams, J.; Han, K.; Spiering, C.] Univ Canterbury, Dept Phys & Astron, Christchurch 1, New Zealand. [Ahrens, J.; Becka, T.; Gozzini, R.; Griesel, T.; Hellwig, M.; Pke, L. Ko; Kowarik, T.; Piegsa, A.] Johannes Gutenberg Univ Mainz, Inst Phys, D-55099 Mainz, Germany. [Andeen, K.; Boersma, D. J.; Braun, J.; Desiati, P.; Diaz-Velez, J. C.; Dumm, J. P.; Ganugapati, R.; Grullon, S.; Halzen, F.; Hanson, K.; Hill, G. C.; Hodges, J.; Hoshina, K.; Hughey, B.; Ishihara, A.; Kappes, A.; Karle, A.; Kelley, J. L.; Kitamura, N.; Krasberg, M.; Landsman, H.; Morse, R.; Oegelman, H.; Schneider, D.; Stamatikos, M.; Strahler, E. A.; Wang, Y. -R.; Wendt, C.; Zornoza, J. D.] Univ Wisconsin, Dept Phys, Madison, WI 53706 USA. [Auffenberg, J.; Becker, K. -H.; Franckowiak, A.; Geenen, H.; Gurtner, M.; Helbing, K.; Kampert, K. -H.; Karg, T.; Robbins, S.; Semburg, B.; Taboada, I.; Tepe, A.; Vandenbroucke, J.] Univ Wuppertal, Dept Phys, D-42119 Wuppertal, Germany. [Bai, X.] Univ Delaware, Bartol Res Inst, Newark, DE 19716 USA. [Baret, B.; De Clercq, C.; Hubert, D.; Labare, M.; Rizzo, A.] Vrije Univ Brussel, Dienst ELEM, B-1050 Brussels, Belgium. [Barwick, S. W.; Gerhardt, L.; Kuehn, K.; Nam, J. W.] Univ Calif Irvine, Dept Phys & Astron, Irvine, CA 92697 USA. [Bay, R.; Filimonov, K.; Hardtke, D.; Morey, A.; Porrata, R.; Price, P. B.] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA. [Beattie, K.; Becker, J. K.; Dreyer, J.; Luenemann, J.; Meli, A.; Messarius, T.; Muenich, K.; Rhode, W.; Wagner, W.] Univ Dortmund, Dept Phys, D-44221 Dortmund, Germany. [Bertrand, D.] Univ Libre Brussels, Fac Sci, B-1050 Brussels, Belgium. [Berley, D.; Blaufuss, E.; Ehrlich, R.; Goodman, J. A.; Hoffman, K. D.; Olivas, A.; Pretz, J.; Roth, P.; Schmidt, T.; Smith, A. J.; Straszheim, T.; Sullivan, G. W.; Turcan, D.] Univ Maryland, Dept Phys, College Pk, MD 20742 USA. [Besson, D. Z.] Univ Kansas, Dept Phys & Astron, Lawrence, KS 66045 USA. [Bohm, C.; Burgess, C.; Burgess, T.; Hulth, P. O.; Hultqvist, K.; Hundertmark, S.; Johansson, H.; Thollander, L.; Walck, C.; Wikstroem, G.] Univ Stockholm, Dept Phys, SE-10691 Stockholm, Sweden. [Botner, O.; Bouchta, A.; Davour, A.; Hallgren, A.; Lundberg, J.; De Los Heros, C. Perez; Pohl, A. C.] Uppsala Univ, Div High Energy Phys, S-75121 Uppsala, Sweden. [Cowen, D. F.; Fox, B. D.; Hart, J. E.; Meszaros, P.; Rutledge, D.; Seo, S. H.; Toale, P. A.; Viscomi, V.; Williams, D. R.] Univ Mons, B-7000 Mons, Belgium. [Hommez, B.; Ryckbosch, D.; Van Overloop, A.] Univ Ghent, Dept Subatom & Radiat Phys, B-9000 Ghent, Belgium. [Eisch, J.; Hardtke, D.; Madsen, J.; Spiczak, G. M.] Univ Wisconsin, Dept Phys, River Falls, WI 54022 USA. [Fadiran, O.] Clark Atlanta Univ, CTSPS, Atlanta, GA 30314 USA. [Fazely, A. R.; Gunasingha, R. M.; Xu, X. W.] So Univ, Dept Phys, Baton Rouge, LA 70813 USA. [Gallagher, J.] Univ Wisconsin, Dept Astron, Madison, WI 53706 USA. [Resconi, E.] Max Planck Inst Kernphys, D-69177 Heidelberg, Germany. [Hasegawa, Y.; Inaba, M.; Kawai, H.; Mase, K.; Miyamoto, H.; Yoshida, S.] Chiba Univ, Dept Phys, Chiba 2638522, Japan. [Huess, J. -P.; Wiebusch, C. H.; Wissing, H.] Rhein Westfal TH Aachen, Inst Phys 3, D-52074 Aachen, Germany. [Kolanoski, H.; Kowalski, M.] Humboldt Univ, Inst Phys, D-12489 Berlin, Germany. [Liubarsky, I.; Sumner, T. J.] Univ London Imperial Coll Sci Technol & Med, Blackett Lab, London SW7 2BW, England. [Pohl, A. C.] Kalmar Univ, Dept Chem & Biomed Sci, S-39182 Kalmar, Sweden. [Sarkar, S.] Univ Oxford, Dept Phys, Oxford OX1 3NP, England. [Zornoza, J. D.] Univ Valencia, CSIC, IFIC, Valencia 46071, Spain. [Boer, M.] Observ Haute Provence, St Michel Observ, F-04870 St Michel, France. [Crew, G.; Ricker, G.] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. [Feroci, M.] CNR, Area Ric Roma Tor Vergata, Inst Nazl Astrofis, Inst Astrofis Spaziale & Fis Cosmica, I-00133 Rome, Italy. [Lamb, D.] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA. [Rau, A.] CALTECH, Caltech Opt Observ, Pasadena, CA 91125 USA. [Von Kienlin, A.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Frontera, F.; Rossi, F.] Univ Ferrara, Dept Phys, I-44100 Ferrara, Italy. [Stamatikos, M.; Cline, T.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Beattie, K.; Goldschmidt, A.; Hays, D.; Jacobsen, J.; Jones, A.; Joseph, J. M.; Klein, S. R.; Matis, H. S.; McParland, C. P.; Nygren, D. R.; Patton, S.; Przybylski, G. T.; Stezelberger, T.; Stokstad, R. G.; Stoufer, M. C.] Lawrence Berkeley Natl Lab, Berkeley, CA 94720 USA. [Rawlins, K.] Univ Alaska Anchorage, Dept Phys & Astron, Anchorage, AK 99508 USA. [Cowen, D. F.; Meszaros, P.; Movit, S. M.; Razzaque, S.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Foerster, M. M.; Fox, B. D.; Hart, J. E.; Seo, S. H.; Viscomi, V.] Penn State Univ, Dept Phys, University Pk, PA 16802 USA. [Bahcall, J. N.] Inst Adv Study, Princeton, NJ 08540 USA. RP Achterberg, A (reprint author), Univ Utrecht, Dept Phys & Astron, NL-3584 CC Utrecht, Netherlands. RI Zornoza, Juan de Dios/L-1604-2014; Sarkar, Subir/G-5978-2011; Song, Chihwa/A-3455-2008; Hundertmark, Stephan/A-6592-2010; Wiebusch, Christopher/G-6490-2012; Kowalski, Marek/G-5546-2012; Botner, Olga/A-9110-2013; Hallgren, Allan/A-8963-2013; Tjus, Julia/G-8145-2012; Auffenberg, Jan/D-3954-2014 OI Hubert, Daan/0000-0002-4365-865X; Zornoza, Juan de Dios/0000-0002-1834-0690; Sarkar, Subir/0000-0002-3542-858X; Perez de los Heros, Carlos/0000-0002-2084-5866; Feroci, Marco/0000-0002-7617-3421; Wiebusch, Christopher/0000-0002-6418-3008; Auffenberg, Jan/0000-0002-1185-9094 NR 65 TC 40 Z9 40 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD FEB 10 PY 2008 VL 674 IS 1 BP 357 EP 370 DI 10.1086/524920 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 266RJ UT WOS:000253454400032 ER PT J AU Christodoulou, DM Contopoulos, I Kazanas, D AF Christodoulou, Dimitris M. Contopoulos, Ioannis Kazanas, Demosthenes TI Simulations of the Poynting-Robertson cosmic battery in resistive accretion disks SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; instabilities; magnetic fields; MHD; plasmas ID RADIATION MAGNETOHYDRODYNAMICS CODE; CONSERVATIVE DIFFERENCE SCHEME; MAGNETIZED COUETTE-FLOW; 2 SPACE DIMENSIONS; ASTROPHYSICAL FLOWS; INTERCHANGE METHOD; BLACK-HOLE; INSTABILITIES; GALAXY; JETS AB We describe the results of numerical "2.5-dimensional'' MHD simulations of an initially unmagnetized disk orbiting a central point mass and responding to the continual generation of poloidalmagnetic field by a secular source emulating the Poynting-Robertson (PR) drag on electrons in the vicinity of a luminous stellar or compact accreting object. The secular PR term has dual purpose both as the magnetic field source and the trigger of magnetorotational instability (MRI). The disk and surrounding hotter atmosphere fluids have finite resistivity, allowing the magnetic field to diffuse out of its generation sites, while at the same time the disk differential rotation twists the poloidal field and induces a substantial toroidal-field component. For moderate disk resistivity (diffusion timescales up to similar to 16 local dynamical times) and after similar to 100 orbits, the MRI allows the fluid of the disk inner edge along with its magnetic flux to flow toward the central point mass where a new, magnetized, nuclear disk forms. The toroidal field in this nuclear disk is amplified by differential rotation and, when near equipartition, unwinds vertically, producing episodic jetlike outflows. For diffusion times longer than the flow time, the poloidal field in the inner region cannot diffuse out; it grows linearly in time, as the outer sections of new poloidal loops are drawn outward by the MRI while their inner sections continue to accumulate onto the compact inner disk. However, for low resistivity (diffusion timescales larger than similar to 16 local dynamical times), the inflowing matter does not form a nuclear disk or jets and the linear growth of the poloidal magnetic field is interrupted after similar to 20 orbits because of magnetic reconnection and asymmetric outflows. C1 [Christodoulou, Dimitris M.] Math Methods, Bedford, MA 01730 USA. [Contopoulos, Ioannis] Acad Athens, Res Ctr Astron, GR-11527 Athens, Greece. [Kazanas, Demosthenes] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Christodoulou, DM (reprint author), Math Methods, 54 Middlesex Turnpike, Bedford, MA 01730 USA. EM dimitris@mathmethods.com; icontop@academyofathens.gr; kazanas@milkyway.gsfc.nasa.gov NR 36 TC 14 Z9 14 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD FEB 10 PY 2008 VL 674 IS 1 BP 388 EP 407 DI 10.1086/524699 PG 20 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 266RJ UT WOS:000253454400035 ER PT J AU Cackett, EM Miller, JM Bhattacharyya, S Grindlay, JE Homan, J Klis, MD Miller, MC Strohmayer, TE Wijnands, R AF Cackett, Edward M. Miller, Jon M. Bhattacharyya, Sudip Grindlay, Jonathan E. Homan, Jeroen Van Der Klis, Michiel Miller, M. Coleman Strohmayer, Tod E. Wijnands, Rudy TI Relativistic iron emission lines in neutron star low-mass X-ray binaries as probes of neutron star radii SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; stars : neutron; X-rays : binaries ID QUASI-PERIODIC OSCILLATIONS; REDSHIFTED ABSORPTION-LINES; FAST-TIME VARIABILITY; EQUATION-OF-STATE; BLACK-HOLE SPIN; GRO J1655-40; BURST SPECTRA; LIGHT CURVES; 4U 1820-30; NGC 6624 AB Using Suzaku observations of three neutron star low-mass X-ray binaries ( Ser X-1, 4U 1820-30, and GX 349+2) we have found broad, asymmetric, relativistic Fe K emission lines in all three objects. These Fe K lines can be well fit by a model for lines from a relativistic accretion disk ("diskline''), allowing a measurement of the inner radius of the accretion disk and hence an upper limit on the neutron star radius. These upper limits correspond to 14.5-16.5 km for a 1.4 M-circle dot neutron star. The inner disk radii that we measure with Fe K lines are in good agreement with the inner disk radii implied by kHz QPOs observed in both 4U 1820-30 and GX 349+2, supporting the inner disk origin for kHz QPOs. In addition, the Fe K lines observed in these neutron stars are narrower than those in the black holes that are thought to be close to maximally spinning, as one would expect if inferences for spin are robust. C1 [Cackett, Edward M.; Miller, Jon M.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Bhattacharyya, Sudip] NASA, Goddard Space Flight Ctr, CRESST & Astrophys Sci Div, Greenbelt, MD 20771 USA. [Bhattacharyya, Sudip; Miller, M. Coleman] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Grindlay, Jonathan E.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Homan, Jeroen] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. [Van Der Klis, Michiel; Wijnands, Rudy] Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1098 SJ Amsterdam, Netherlands. [Strohmayer, Tod E.] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA. RP Cackett, EM (reprint author), Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. EM ecackett@umich.edu RI XRAY, SUZAKU/A-1808-2009 NR 54 TC 72 Z9 72 U1 0 U2 1 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 FEB 10 PY 2008 VL 674 IS 1 BP 415 EP 420 DI 10.1086/524936 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 266RJ UT WOS:000253454400037 ER PT J AU Swain, MR Bouwman, J Akeson, RL Lawler, S Beichman, CA AF Swain, M. R. Bouwman, J. Akeson, R. L. Lawler, S. Beichman, C. A. TI The mid-infrared spectrum of the transiting exoplanet HD 209458b SO ASTROPHYSICAL JOURNAL LA English DT Article DE methods : data analysis; planetary systems; stars : individual (HD 209458); techniques : spectroscopic ID SPITZER-SPACE-TELESCOPE; SOLAR-TYPE STARS; EXTRASOLAR PLANET; INFRARED SPECTROGRAPH; SECONDARY ECLIPSE; SEARCH; EMISSION; 189733B; IRS AB We report the spectroscopic detection of mid-infrared emission from the transiting exoplanet HD 209458b. Using archive data taken with the Spitzer IRS instrument, we have determined the spectrum of HD 209458b between 7.46 and 15.25 mu m. We have used two independent methods to determine the planet spectrum, one differential in wavelength and one absolute, and find the results are in good agreement. Over much of this spectral range, the planet spectrum is consistent with featureless thermal emission. Between 7.5 and 8.5 mu m, we find evidence for an unidentified spectral feature. If this spectral modulation is due to absorption, it implies that the dayside vertical temperature profile of the planetary atmosphere is not entirely isothermal. Using the IRS data, we have determined the broadband eclipse depth to be 0: 00315 +/- 0: 000315, implying significant redistribution of heat from the dayside to the nightside. This work required the development of improved methods for Spitzer IRS data calibration that increase the achievable absolute calibration precision and dynamic range for observations of bright point sources. C1 [Swain, M. R.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Bouwman, J.] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Akeson, R. L.; Lawler, S.; Beichman, C. A.] CALTECH, Michelson Sci Ctr, Pasadena, CA 91125 USA. RP Swain, MR (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. NR 22 TC 64 Z9 65 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 FEB 10 PY 2008 VL 674 IS 1 BP 482 EP 497 DI 10.1086/523832 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 266RJ UT WOS:000253454400043 ER PT J AU Gopalswamy, N Yashiro, S Xie, H Akiyama, S Aguilar-Rodriguez, E Kaiser, ML Howard, RA Bougeret, JL AF Gopalswamy, N. Yashiro, S. Xie, H. Akiyama, S. Aguilar-Rodriguez, E. Kaiser, M. L. Howard, R. A. Bougeret, J. -L. TI Radio-quiet fast and wide coronal mass ejections SO ASTROPHYSICAL JOURNAL LA English DT Article DE solar-terrestrial relations; Sun : corona; Sun : coronal mass ejections (CMEs); Sun : flares; Sun : particle emission; Sun : radio radiation ID ENERGETIC PARTICLE EVENTS; LARGE-ANGLE; SOLAR; SPACECRAFT; BURSTS; WAVES; SHOCK; SUN AB We report on the properties of radio-quiet (RQ) and radio-loud (RL) coronal mass ejections (CMEs) that are fast and wide (FW). RQ CMEs lack type II radio bursts in the metric and decameter-hectometric (DH) wavelengths. RL CMEs are associated with metric or DH type II bursts. We found that similar to 40% of the FW CMEs from 1996 to 2005 were RQ. The RQ CMEs had an average speed of 1117 km s(-1) compared to 1438 km s(-1) for the RL, bracketing the average speed of all FW CMEs (1303 km s(-1)). The fraction of full halo CMEs (apparent width 360 degrees) was the largest for the RL CMEs (60%), smallest for the RQ CMEs (16%), and intermediate for all FW CMEs (42%). The median soft X-ray flare size for the RQ CMEs (C6.9) was also smaller than that for the RL CMEs (M3.9). About 55% of RQ CMEs were back sided, while the front-sided ones originated close to the limb. The RL CMEs originated generally on the disk with only similar to 25% being back sided. The RQ FW CMEs suggest that the Alfven speed in the low-latitude outer corona can often exceed 1000 km s(-1) and can vary over a factor of >= 3. None of the RQ CMEs was associated with large solar energetic particle events, which is useful information for space weather applications. C1 [Gopalswamy, N.; Kaiser, M. L.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Yashiro, S.; Xie, H.; Akiyama, S.; Aguilar-Rodriguez, E.] Catholic Univ Amer, Washington, DC 20064 USA. [Howard, R. A.] USN, Res Lab, Washington, DC 20375 USA. [Bougeret, J. -L.] Observ Paris, Meudon, France. RP Gopalswamy, N (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RI Gopalswamy, Nat/D-3659-2012; OI Gopalswamy, Nat/0000-0001-5894-9954 NR 25 TC 47 Z9 47 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 FEB 10 PY 2008 VL 674 IS 1 BP 560 EP 569 DI 10.1086/524765 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 266RJ UT WOS:000253454400050 ER PT J AU Wang, AH Wu, ST Liu, Y Hathaway, D AF Wang, A. H. Wu, S. T. Liu, Yang Hathaway, D. TI Recovering photospheric velocities from vector magnetograms by using a three-dimensional, fully magnetohydrodynamic model SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE MHD; Sun : activity; Sun : atmospheric motions; Sun : magnetic fields ID PROJECTED CHARACTERISTICS; MAGNETIC-FIELDS; ACTIVE-REGION; EVOLUTION; ENERGY; FLARES; RECONSTRUCTION; FORMULATION; TRACKING; MOTION AB We use a numerical simulation method for recovering the photospheric velocity field from the vector magnetograms. The traditional method is local correlation tracking (LCT), which is based on measuring the relative displacements of features in blocks of pixels between successive white-light images or magnetograms. Within this method, there are a variety of implementations. One of recently developed implementations is induction local correlation tracking (ILCT) as described by Welsch and coworkers. They employ the normal component of magnetic induction equation as a constraint to assure consistent solutions. Our numerical method uses the fully three-dimensional MHD equations to recover the photospheric velocity field with individual vector magnetograms. We compare our method to the ILCT method using NOAA AR 8210 as an example. The differences and similarities are discussed in detail. C1 [Wang, A. H.; Wu, S. T.] Univ Alabama, Ctr Space Plasma & Aeronom Res, Huntsville, AL 35899 USA. [Wang, A. H.; Wu, S. T.] Univ Alabama, Dept Mech & Aerosp Engn, Huntsville, AL 35899 USA. [Liu, Yang] Stanford Univ, WW Hansen Expt Phys Lab, Stanford, CA 94305 USA. [Hathaway, D.] NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA. RP Wang, AH (reprint author), Univ Alabama, Ctr Space Plasma & Aeronom Res, Huntsville, AL 35899 USA. NR 22 TC 8 Z9 8 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD FEB 10 PY 2008 VL 674 IS 1 BP L57 EP L60 DI 10.1086/528844 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 291YT UT WOS:000255234100015 ER PT J AU Freund, FT AF Freund, Friedemann T. TI Earthquake probabilities and pre-earthquake signals SO CURRENT SCIENCE LA English DT Article ID EMISSIONS; ANOMALIES; ROCKS C1 [Freund, Friedemann T.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Freund, FT (reprint author), NASA, Ames Res Ctr, MS 242-4, Moffett Field, CA 94035 USA. EM friedemann.t.freund@nasa.gov NR 20 TC 2 Z9 2 U1 0 U2 3 PU CURRENT SCIENCE ASSOC PI BANGALORE PA C V RAMAN AVENUE, PO BOX 8005, BANGALORE 560 080, INDIA SN 0011-3891 J9 CURR SCI INDIA JI Curr. Sci. PD FEB 10 PY 2008 VL 94 IS 3 BP 311 EP 313 PG 3 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 264UJ UT WOS:000253315600017 ER PT J AU Howard, AD Moore, JM AF Howard, Alan D. Moore, Jeffrey M. TI Sublimation-driven erosion on Callisto: A landform simulation model test SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID GALILEAN SATELLITES; DEGRADATION; SURFACE; ATMOSPHERE; MORPHOLOGY; EVOLUTION AB Callisto's landscape exhibits widespread erosion from some non-impact-induced process, which is characterized by smooth, undulating dark albedo surfaces with isolated high albedo knobs that are remnants of crater rims. We develop a landform simulation model that incorporates sublimation erosion of exposed bedrock on crater walls, composed of ice-cemented dust, with non-linear mass wasting of the released dust and redeposition of the ice on convex summits. The model reproduces the essential elements of landscapes on Callisto, and lends strong support to the 1999 hypothesis of Moore and his colleagues that volatile sublimation causes slope-forming bedrock disaggregation and subsequent mass wasting while reprecipitation caps and armors local crests with frost. C1 [Howard, Alan D.] Univ Virginia, Dept Environm Sci, Charlottesville, VA 22903 USA. [Moore, Jeffrey M.] NASA, Ames Res Ctr, Div Space Sci, Moffett Field, CA 94035 USA. RP Howard, AD (reprint author), Univ Virginia, Dept Environm Sci, 1156 High St, Charlottesville, VA 22903 USA. EM jeff.moore@nasa.gov OI Howard, Alan/0000-0002-5423-1600 NR 21 TC 5 Z9 5 U1 0 U2 3 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD FEB 9 PY 2008 VL 35 IS 3 AR L03203 DI 10.1029/2007GL032618 PG 4 WC Geosciences, Multidisciplinary SC Geology GA 261FK UT WOS:000253064300004 ER PT J AU Grodsky, SA Carton, JA McClain, CR AF Grodsky, Semyon A. Carton, James A. McClain, Charles R. TI Variability of upwelling and chlorophyll in the equatorial Atlantic SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID TROPICAL ATLANTIC; SEASONAL CYCLE; OCEAN; PROJECT; MODEL AB The primary seasonal phytoplankton bloom in the equatorial Atlantic occurs in boreal summer in response to seasonal strengthening of zonal winds. However, the equatorial Atlantic also has a secondary bloom in late fall - early winter. This secondary bloom is weaker than the primary bloom by a factor of two, but is subject to year-to-year variability that is similar in magnitude. Here, observational evidence, including sea level and SeaWiFS-derived chlorophyll-a concentration, is used to examine several potential causes of this secondary bloom. The secondary bloom varies independently of blooms along the eastern coastal zones. Also, the secondary bloom has a relationship with the cessation of the Northwest African monsoon, which propotes the secondary seasonal strengthening of the trade winds. The variability of the secondary bloom results from perturbations in the depth of the thermocline induced by zonal wind anomalies in the western tropical Atlantic. These wind anomalies are correlated with mean sea level atmospheric pressure anomalies in the region of the northern subtropical high as well as over the Amazon. C1 [Grodsky, Semyon A.; Carton, James A.] Univ Maryland, Dept Atmospher & Ocean Sci, College Pk, MD 20742 USA. [McClain, Charles R.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Grodsky, SA (reprint author), Univ Maryland, Dept Atmospher & Ocean Sci, College Pk, MD 20742 USA. RI carton, james/C-4807-2009; Grodsky, Semyon/F-4929-2010 OI carton, james/0000-0003-0598-5198; Grodsky, Semyon/0000-0002-0670-1356 NR 18 TC 15 Z9 15 U1 2 U2 14 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 FEB 8 PY 2008 VL 35 IS 3 AR L03610 DI 10.1029/2007GL032466 PG 6 WC Geosciences, Multidisciplinary SC Geology GA 261FH UT WOS:000253064000001 ER EF