FN Thomson Reuters Web of Science™ VR 1.0 PT J AU Dyudina, UA Ingersoll, AP Ewald, SP Vasavada, AR West, RA Baines, IH Momary, TW Del Genio, AD Barbara, JM Porco, CC Achterberge, RK Flasar, FM Simon-Miller, AA Fletcher, LN AF Dyudina, Ulyana A. Ingersoll, Andrew P. Ewald, Shawn P. Vasavada, Ashwin R. West, Robert A. Baines, Ievin H. Momary, Thomas W. Del Genio, Anthony D. Barbara, John M. Porco, Carolyn C. Achterberge, Richard K. Flasar, F. Michael Simon-Miller, Amy A. Fletcher, Leigh N. TI Saturn's south polar vortex compared to other large vortices in the Solar System SO ICARUS LA English DT Article DE Saturn, atmosphere; Atmospheres, dynamics; Infrared observations; Meteorology; Spectroscopy ID GREAT RED SPOT; ATMOSPHERE; DYNAMICS; CASSINI; TEMPERATURE; FIELD AB Observations made by the Imaging Science Subsystem (ISS), Visible and infrared Mapping Spectrometer (VIMS) and the long-wavelength Composite infrared Spectrometer (CIRS) aboard the Cassini spacecraft reveal that the large, long-lived cyclonic vortex at Saturn's south pole has a 4200-km-diameter cloud-free nearly circular region. This region has a 4 K warm core extending from the troposphere into the stratosphere, concentric cloud walls extending 20-70 km above the internal Clouds, and numerous external clouds whose anticyclonic vorticity suggests a convective origin. The rotation speeds of the vortex reach 150 +/- 20 ms(-1). The Saturn polar vortex has features in common with terrestrial hurricanes and with the Venus polar vortex. Neptune and other giant planets may also have strong polar vortices. (C) 2009 Elsevier Inc. All rights reserved. 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.; Baines, Ievin H.; Momary, Thomas W.; 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, Cassini Imaging Cent Lab Operat, Boulder, CO 80301 USA. [Achterberge, Richard K.; Flasar, F. Michael; Simon-Miller, Amy A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. 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 FU NASA FX This research was supported by the NASA Cassini Project. NR 26 TC 21 Z9 21 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 EI 1090-2643 J9 ICARUS JI Icarus PD JUL PY 2009 VL 202 IS 1 BP 240 EP 248 DI 10.1016/j.icarus.2009.02.014 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 460ZD UT WOS:000267231000019 ER PT J AU Hesman, BE Jennings, DE Sada, PV Bjoraker, GL Achterberg, RK Simon-Miller, AA Anderson, CM Boyle, RJ Nixon, CA Fletcher, LN McCabe, GH AF Hesman, Brigette E. Jennings, Donald E. Sada, Pedro V. Bjoraker, Gordon L. Achterberg, Richard K. Simon-Miller, Amy A. Anderson, Carrie M. Boyle, Robert J. Nixon, Conor A. Fletcher, Leigh N. McCabe, George H. TI Saturn's latitudinal C2H2 and C2H6 abundance profiles from Cassini/CIRS and ground-based observations SO ICARUS LA English DT Article DE Abundances, atmospheres; Saturn, atmosphere; Atmospheres, dynamics ID ROTOTRANSLATIONAL ABSORPTION-SPECTRA; OUTER PLANETS; MERIDIONAL VARIATIONS; STRATOSPHERE; TEMPERATURE; ATMOSPHERE; PAIRS; SYSTEM; MODEL AB Hydrocarbons in the upper atmosphere of Saturn are known, from Voyager, ground-based, and early Cassini results, to vary in emission intensity with latitude. Of particular interest is the marked increase in hydrocarbon line intensity near the south pole during southern summer, as the increased line intensity cannot be simply explained by the increased temperatures observed in that region since the variations between C2H2 and C2H6 emission in the south pole region are different. In order to measure the latitudinal variations of hydrocarbons in Saturn's southern hemisphere we have used 3 cm(-1) resolution Cassini CIRS data from 2006 and combined this with measurements from the ground in October 2006 at NASA's IRTF using Celeste, an infrared high-resolution cryogenic grating spectrometer. These two data sets have been used to infer the molecular abundances Of C2H2 and C2H6 across the southern hemisphere in the 1-10 mbar altitude region. We find that the latitudinal acetylene profile follows the yearly average mean daily insolation except at the southern pole where it peaks in abundance. Near the equator (5 degrees S) the C2H2 abundance at the 1.2 mbar level is (1.6 +/- 0.19) x 10(-7) and it decreases by a factor of 2.7 from the equator toward the pole. However, at the pole (similar to 87 degrees S) the C2H2 abundance jumps to (1.8 +/- 0.3) x 10(-7), approximately the equatorial value. The C2H6 abundance near the equator at the 2 mbar level is (0.7 +/- 0.1) x 10(-5) and stays approximately constant until mid-latitudes where it increases gradually toward the pole, attaining a value of (1.4 +/- 0.4) x 10(-5) there. The increase in ethane toward the pole with the corresponding decrease in acetylene is consistent with southern hemisphere meridional winds [Greathouse, TIC, Lacy, J.H., Bezard, B., Moses, J.I., Griffith, C.A., Richter, M.J., 2005. Icarus 177, 18-31]. The localized increase in acetylene at the pole provides evidence that there is dynamical transport of hydrocarbons from the equator to the southern pole. (C) 2009 Elsevier Inc. All rights reserved. C1 [Hesman, Brigette E.] Natl Radio Astron Observ, Pete V Domenici Sci Operat Ctr, Socorro, NM 87801 USA. [Jennings, Donald E.; Bjoraker, Gordon L.; Simon-Miller, Amy A.; Anderson, Carrie M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Sada, Pedro V.] Univ Monterrey, Dept Fis Math, Garza Garcia 66238, NL, Mexico. [Achterberg, Richard K.; Nixon, Conor A.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Boyle, Robert J.] Dickinson Coll, Dept Phys & Astron, Carlisle, PA 17013 USA. [Fletcher, Leigh N.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [McCabe, George H.] CMA Consulting Serv, Latham, NY 12110 USA. RP Hesman, BE (reprint author), Natl Radio Astron Observ, Pete V Domenici Sci Operat Ctr, 1003 Lopezville Rd, Socorro, NM 87801 USA. EM bhesman@aoc.nrao.edu RI Fletcher, Leigh/D-6093-2011; Nixon, Conor/A-8531-2009; Anderson, Carrie/C-8097-2012; Bjoraker, Gordon/D-5032-2012; Jennings, Donald/D-7978-2012; Simon, Amy/C-8020-2012 OI Fletcher, Leigh/0000-0001-5834-9588; Nixon, Conor/0000-0001-9540-9121; Simon, Amy/0000-0003-4641-6186 FU NASA; National Radio Astronomy Observatory FX The authors wish to thank the NASA Infrared Telescope staff for their assistance during the observations. The Cassini/CIRS team is recognized for their work in sequence planning, data reduction, and calibration. This research was supported in part by the NASA Planetary Astronomy Program. BE Hesman was supported by a NASA Postdoctoral Program Fellowship appointment conducted at the Goddard Space Flight Center, administered by Oak Ridge Associated Universities through a contract with NASA. BE Hestnan is currently supported by the National Radio Astronomy Observatory. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Incorporated. D.E.J., G.L.B., RKA., A.A.S.-M., and C.A.N. acknowledge the continuing support of the NASA Cassini Mission. C.M. Anderson was supported by an appointment to the NASA Postdoctoral Program at the Goddard Space Flight Center, administered by Oak Ridge Associated Universities through a contract with NASA. L.N. Fletcher was supported by an appointment to the NASA Postdoctoral Program at the jet Propulsion Laboratory, California Institute of Technology, administered by Oak Ridge Associated Universities through a contract with NASA. NR 25 TC 20 Z9 20 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 EI 1090-2643 J9 ICARUS JI Icarus PD JUL PY 2009 VL 202 IS 1 BP 249 EP 259 DI 10.1016/j.icarus.2009.02.013 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 460ZD UT WOS:000267231000020 ER PT J AU Martinelli, LK Russomano, T Dos Santos, MA Falcao, FP Bauer, ME Machado, A Sundaresan, A AF Martinelli, Leonardo K. Russomano, Thais Dos Santos, Marlise A. Falcao, Felipe P. Bauer, Moises E. Machado, Amanda Sundaresan, Alamelu TI Effect of Microgravity on Immune Cell Viability and Proliferation Simulation Using 3-D Clinostat SO IEEE ENGINEERING IN MEDICINE AND BIOLOGY MAGAZINE LA English DT Article ID SPACEFLIGHT; CLINOROTATION; ACTIVATION; RESPONSES C1 [Martinelli, Leonardo K.] Pontificia Univ Catolica Rio Grande do Sul, Micrograv Ctr, FENG, BR-90619900 Porto Alegre, RS, Brazil. [Sundaresan, Alamelu] NASA, JSC, Cellular Movement & Signal Transduct Lab, Washington, DC USA. [Sundaresan, Alamelu] Univ Texas Hlth Sci Ctr Houston, Houston, TX USA. RP Martinelli, LK (reprint author), Pontificia Univ Catolica Rio Grande do Sul, Micrograv Ctr, FENG, Bldg 30,Block F,Room 216,Av Ipiranga 6681, BR-90619900 Porto Alegre, RS, Brazil. EM microg@pucrs.br RI Bauer, Moises/J-9195-2015 OI Bauer, Moises/0000-0003-2957-1352 NR 18 TC 5 Z9 8 U1 0 U2 2 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 0739-5175 J9 IEEE ENG MED BIOL JI IEEE Eng. Med. Biol. Mag. PD JUL-AUG PY 2009 VL 28 IS 4 BP 85 EP 90 DI 10.1109/MEMB.2009.933572 PG 6 WC Engineering, Biomedical; Medical Informatics SC Engineering; Medical Informatics GA 474KJ UT WOS:000268281900019 PM 19622430 ER PT J AU Mackenzie, AI Rao, SM Baginski, ME AF Mackenzie, Anne I. Rao, Sadasiva M. Baginski, Michael E. TI Electromagnetic Scattering From Arbitrarily Shaped Dielectric Bodies Using Paired Pulse Vector Basis Functions and Method of Moments SO IEEE TRANSACTIONS ON ANTENNAS AND PROPAGATION LA English DT Article DE Basis functions; boundary integral equations; conducting materials; dielectric materials; electromagnetic scattering; method of moments (MoM) ID FORMULATION; REVOLUTION; OBJECTS; FIELD AB A pair of orthogonal pulse vector basis functions is demonstrated for the calculation of electromagnetic scattering from arbitrarily-shaped material bodies. The basis functions are intended for use with triangular surface patch modeling applied to a method of moments (MoM) solution. For modeling the behavior of dielectric materials, several authors have used the same set of basis functions to represent equivalent electric and magnetic surface currents. This practice can result in zero-valued or very small diagonal terms in the moment matrix and an unstable numerical solution. To provide a more stable solution, we have developed orthogonally placed, pulse basis vectors: one for the electric surface current and one for the magnetic surface current. This combination ensures strongly diagonal moment matrices. The basis functions are suitable for electric field integral equation (EFIE), magnetic field integral equation (HFIE), and combined field formulations. In this work, we describe the implementations for EFIE and HFIE formulations and show example results for canonical figures. C1 [Mackenzie, Anne I.] NASA, Langley Res Ctr, Electromagnet & Sensors Branch, Hampton, VA 23681 USA. [Rao, Sadasiva M.; Baginski, Michael E.] Auburn Univ, Dept Elect & Comp Engn, Auburn, AL 36849 USA. RP Mackenzie, AI (reprint author), NASA, Langley Res Ctr, Electromagnet & Sensors Branch, Hampton, VA 23681 USA. EM anne.mackenzie-1@nasa.gov NR 12 TC 6 Z9 6 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 JUL PY 2009 VL 57 IS 7 BP 2076 EP 2083 DI 10.1109/TAP.2009.2021891 PG 8 WC Engineering, Electrical & Electronic; Telecommunications SC Engineering; Telecommunications GA 471ES UT WOS:000268039000023 ER PT J AU de Matthaeis, P Lang, RH AF de Matthaeis, Paolo Lang, Roger H. TI Comparison of Surface and Volume Currents Models for Electromagnetic Scattering From Finite Dielectric Cylinders SO IEEE TRANSACTIONS ON ANTENNAS AND PROPAGATION LA English DT Article DE Dielectric cylinders; electromagnetic scattering; remote sensing ID VEGETATION AB The accuracy of modeling plane wave scattering by dielectric cylinders of finite length and circular cross section for microwave remote sensing applications is investigated. Exact expressions for their scattering cross section do not exist, leading to the use of approximate analytical methods. Two widely used models, based on the approximation of the induced currents, are considered here, and the validity of their results is evaluated by comparison with a corresponding numerical solution. C1 [de Matthaeis, Paolo] NASA, Goddard Earth Sci & Technol Ctr, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Lang, Roger H.] George Washington Univ, Dept Elect & Comp Engn, Washington, DC 20052 USA. RP de Matthaeis, P (reprint author), NASA, Goddard Earth Sci & Technol Ctr, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. EM paolo.dematthaeis@nasa.gov NR 12 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 0018-926X J9 IEEE T ANTENN PROPAG JI IEEE Trans. Antennas Propag. PD JUL PY 2009 VL 57 IS 7 BP 2216 EP 2220 DI 10.1109/TAP.2009.2021977 PG 5 WC Engineering, Electrical & Electronic; Telecommunications SC Engineering; Telecommunications GA 471ES UT WOS:000268039000044 ER PT J AU Daigle, MJ Koutsoukos, XD Biswas, G AF Daigle, Matthew J. Koutsoukos, Xenofon D. Biswas, Gautam TI A Qualitative Event-Based Approach to Continuous Systems Diagnosis SO IEEE TRANSACTIONS ON CONTROL SYSTEMS TECHNOLOGY LA English DT Article DE Discrete-event system (DES); electrical power systems; model-based diagnosis ID LEAD-ACID-BATTERIES; FAULT-DIAGNOSIS; FAILURE DIAGNOSIS; DYNAMICAL MODELS; BOND GRAPHS; DISCRETE AB Fault diagnosis is crucial for ensuring the safe operation of complex engineering systems. Although discrete-event diagnosis methods are used extensively, they do not easily address parametric fault isolation in systems with complex continuous dynamics. This paper presents a novel event-based approach for diagnosis of abrupt parametric faults in continuous systems, based on a qualitative abstraction of measurement deviations from the nominal behavior. From a continuous model of the system, we systematically derive dynamic fault signatures expressed as event-based fault models, which are used, in turn, for designing an event-based diagnoser of the system and determining system diagnosability. The proposed approach is applied to a subset of the Advanced Diagnostics and Prognostics Testbed, which is representative of a spacecraft's electrical power system. We present experimental results from the actual testbed, as well as detailed simulation experiments that examine the performance of our diagnosis algorithms under different fault magnitudes and noise levels. C1 [Daigle, Matthew J.] Univ Calif Santa Cruz, NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Koutsoukos, Xenofon D.; Biswas, Gautam] Vanderbilt Univ, Dept Elect Engn & Comp Sci, Inst Software Integrated Syst, Nashville, TN 37235 USA. RP Daigle, MJ (reprint author), Univ Calif Santa Cruz, NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. EM matthew.j.daigle@nasa.gov; xenofon.koutsoukos@vanderbilt.edu; gautam.biswas@vanderbilt.edu OI Daigle, Matthew/0000-0002-4616-3302 NR 42 TC 13 Z9 13 U1 0 U2 7 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 1063-6536 EI 1558-0865 J9 IEEE T CONTR SYST T JI IEEE Trans. Control Syst. Technol. PD JUL PY 2009 VL 17 IS 4 BP 780 EP 793 DI 10.1109/TCST.2008.2011648 PG 14 WC Automation & Control Systems; Engineering, Electrical & Electronic SC Automation & Control Systems; Engineering GA 463MI UT WOS:000267435900004 ER PT J AU Kokhanovsky, AA Naud, CM Devasthale, A AF Kokhanovsky, Alexander A. Naud, Catherine M. Devasthale, Abhay TI Intercomparison of Ground-Based Radar and Satellite Cloud-Top Height Retrievals for Overcast Single-Layered Cloud Fields SO IEEE TRANSACTIONS ON GEOSCIENCE AND REMOTE SENSING LA English DT Article DE Clouds; radiative transfer; remote sensing ID MODIS; ALTITUDES; REFLECTANCE; INSTRUMENTS; RADIATION; PRESSURE; SYSTEM; MISR; GOME AB The objective of this paper is to assess the accuracy of the Semi-Analytical CloUd Retrieval Algorithm (SACURA) that retrieves cloud-top heights (CTHs) using hyperspectral SCanning Imaging Absorption spectroMeter for Atmospheric CHartographY (SCIAMACHY) onboard Environmental Satellite measurements for overcast single-layer cloud fields. Intercomparisons with ground-based 35-GHz millimeter wave cloud radar CTHs were performed for 14 dates during 2003-2007 at the US. Atmospheric Radiation Measurement (ARM) program Southern Great Plains site (36.6 degrees N, 97.5 degrees W). In addition, for some of these dates, European Space Agency MEdium Resolution Imaging Spectrometer (MERIS) and the NASAL-TERRA Moderate Resolution Imaging Spectroradiometer (MODIS) cloud-top pressure retrievals were also collected, transformed into CTHs using nearby ARM radiosonde profiles, and compared with the SACURA SCIAMACHY and radar retrievals. The accuracy of the SACURA-SCIAMACHY CTH retrievals is better than 0.34 km for low-level clouds and 2.22 km for high-level clouds with an underestimate in CTH on average for all clouds. The average bias in SCIAMACHY CTHs was about 0.07 km for low clouds and about 0.5 km for high-level clouds. Both MODIS and MERIS slightly overestimated the CTHs of low-level clouds by MO m, with an uncertainty better than 1 km. However, although MODIS accuracy for high-level clouds is close to SCIAMACHY, MERIS CTHs were significantly underestimated for these fairly optically thick cases. C1 [Kokhanovsky, Alexander A.] Univ Bremen, Inst Environm Phys, D-28334 Bremen, Germany. [Naud, Catherine M.] Columbia Univ, Dept Appl Phys & Appl Math, New York, NY 10025 USA. [Naud, Catherine M.] NASA Goddard Inst Space Studies, New York, NY 10025 USA. [Devasthale, Abhay] Swedish Meteorol & Hydrol Inst, S-60176 Norrkoping, Sweden. RP Kokhanovsky, AA (reprint author), Univ Bremen, Inst Environm Phys, D-28334 Bremen, Germany. EM alexk@iupphysik.uni-bremen.de; cn2140@columbia.edu; Abhay.Devasthale@smhi.se RI Kokhanovsky, Alexander/C-6234-2016; OI Kokhanovsky, Alexander/0000-0001-7370-1164; Devasthale, Abhay/0000-0002-6717-8343 FU German Space Agency (DLR); European Space Agency (ESA); German Science Foundation (DFG) FX This work was Supported in part by the German Space Agency (DLR), by the European Space Agency (ESA), and by the German Science Foundation (DFG). NR 22 TC 5 Z9 5 U1 0 U2 3 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 JUL PY 2009 VL 47 IS 7 BP 1901 EP 1908 DI 10.1109/TGRS.2008.2010455 PN 1 PG 8 WC Geochemistry & Geophysics; Engineering, Electrical & Electronic; Remote Sensing; Imaging Science & Photographic Technology SC Geochemistry & Geophysics; Engineering; Remote Sensing; Imaging Science & Photographic Technology GA 463MV UT WOS:000267437200002 ER PT J AU Cossio, T Slatton, KC Carter, W Shrestha, K Harding, D AF Cossio, Tristan Slatton, K. Clint Carter, William Shrestha, Kris Harding, David TI Predicting Topographic and Bathymetric Measurement Performance for Low-SNR Airborne Lidar SO IEEE TRANSACTIONS ON GEOSCIENCE AND REMOTE SENSING LA English DT Article DE Bathymetry; light detection and ranging (lidar); photonics; simulation ID LASER ALTIMETERS; OCEAN SURFACE; BACKSCATTER; REFLECTANCE; SCATTERING; WHITECAPS; TARGET AB Government and commercial airborne light detection and ranging (lidar) systems have enabled extensive measurements of the Earth's surface and land cover over the past decade. There is much interest, however, in employing smaller lidar systems that require less power to enable sensing from small unmanned aerial vehicles or satellites. Technological advances in the performance of small microlasers and photodetector sensitivity have recently enabled the development of experimental airborne lidar systems with low signal-to-noise ratios (LSNRs). Recent government and academic prototypes have indicated that LSNR airborne lidars could significantly increase the fidelity of terrain reconstruction over what is possible with existing conventional lidars. Thus, there is a need to build up a modeling capability for such systems in order to aid in future system and mission design. A numerical sensor simulator has been developed to model the expected returns from LSNR microlaser altimeter systems and predict their performance. Both optical and signal processing system components are considered, along with other factors, including atmospheric effects and surface conditions. Topographic (solid Earth) and bathymetric (littoral zone) measurement scenarios are considered. The analysis of topographic simulation data focuses on the effect of solar noise on SNR and elevation accuracy while bathymetric performance is evaluated with regard to water depth and scan angle for different water clarities. The mission conditions chiefly responsible for limiting the performance of LSNR lidar are discussed in detail, along with suggestions for further algorithm development and system performance evaluation. C1 [Cossio, Tristan; Slatton, K. Clint] Univ Florida, Dept Elect & Comp Engn, Adapt Signal Proc Lab, Gainesville, FL 32611 USA. [Slatton, K. Clint] Univ Florida, Natl Ctr Airborne Laser Mapping, Dept Civil & Coastal Engn, Gainesville, FL 32611 USA. [Harding, David] NASA, Goddard Space Flight Ctr, Planetary Geodynam Lab, Sci & Explorat Directorate, Greenbelt, MD 20771 USA. RP Cossio, T (reprint author), Univ Florida, Dept Elect & Comp Engn, Adapt Signal Proc Lab, Gainesville, FL 32611 USA. EM tcossio@ecel.ufl.edu; slatton@ece.ufl.edu; bcarter@ce.ufl.edu; kshres@gmail.com; David.J.Harding@nasa.gov RI Harding, David/F-5913-2012 FU NASA Graduate Student Researchers Program; National Science Foundation's National Center for Airborne Laser Mapping FX The work of T. Cossio was supported in part by a NASA Graduate Student Researchers Program fellowship and in part by the National Science Foundation's National Center for Airborne Laser Mapping. NR 45 TC 18 Z9 18 U1 1 U2 16 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 0196-2892 J9 IEEE T GEOSCI REMOTE JI IEEE Trans. Geosci. Remote Sensing PD JUL PY 2009 VL 47 IS 7 BP 2298 EP 2315 DI 10.1109/TGRS.2008.2011054 PN 2 PG 18 WC Geochemistry & Geophysics; Engineering, Electrical & Electronic; Remote Sensing; Imaging Science & Photographic Technology SC Geochemistry & Geophysics; Engineering; Remote Sensing; Imaging Science & Photographic Technology GA 463MW UT WOS:000267437300019 ER PT J AU Krishen, K AF Krishen, Kumar TI Technology Needs for Future Space Exploration SO IETE TECHNICAL REVIEW LA English DT Article DE Space exploration; Technology needs; Human missions; Moon; Mars; Low-earth-orbit; Geostationary orbit; In-situ resources; Resource reuse; Safety; Human support AB Human exploration and development of space is aimed at opening the space frontier by exploring, using, and enabling the development of space and expanding the human experience into the far reaches of space. This includes increasing human knowledge of nature's processes using the space environment, exploring and settling the solar system, achieving routine space travel, and enriching life on Earth through people living and working in space. NASA's Mars robotic explorations and the International Space Station provide extensive experience, research and technology (R&T), and infrastructure for other envisioned programs in support of human exploration and development of space. The missions to Moon by United States, Russia, China, India, and Japan have provided valuable data for the Moon. In addition, NASA has studied the development of a lunar habitat and human mission to Mars as possible future missions. These missions face common challenges of travel to these planets and for the survival of humans on the surface of the planets. With the human Mars mission being the first to such a distant planet, advanced technologies will be required to enable the mission and to provide cost effective and safer approaches. The R&T areas considered important for future human mission include advanced human support, renewable resources and utilization of planetary resources, space transportation, automation and robotics, space power, information processing and communications systems, sensors, and instruments. C1 NASA, Lyndon B Johnson Space Ctr, Innovat Partnerships Off, Houston, TX 77058 USA. RP Krishen, K (reprint author), NASA, Lyndon B Johnson Space Ctr, Innovat Partnerships Off, 2101 NASA Pkwy, Houston, TX 77058 USA. EM krishen59@gmail.com NR 8 TC 2 Z9 2 U1 2 U2 14 PU INST ELECTRONICS TELECOMMUNICATION ENGINEERS PI NEW DELHI PA 2 INSTITUTIONAL AREA, LODI ROAD, NEW DELHI 110 003, INDIA SN 0256-4602 J9 IETE TECH REV JI IETE Tech. Rev. PD JUL-AUG PY 2009 VL 26 IS 4 BP 228 EP 235 DI 10.4103/0256-4602.52992 PG 8 WC Engineering, Electrical & Electronic; Telecommunications SC Engineering; Telecommunications GA 468JJ UT WOS:000267813400002 ER PT J AU Panzarella, C Kassemi, M AF Panzarella, Charles Kassemi, Mohammad TI One-dimensional model of evaporation and condensation in the presence of a noncondensable gas with applications to cryogenic fluid storage SO INTERNATIONAL JOURNAL OF HEAT AND MASS TRANSFER LA English DT Article DE Evaporation; Condensation; Noncondensable; Two-phase flow; Cryogenic storage; Zero boil off ID KINETIC-THEORY; VAPOR FLOWS; LIQUID; EXPRESSION AB This paper considers the one-dimensional flow of vapor between two liquid surfaces due to evaporation and condensation taking into account diffusion through a noncondensable gas and nonequilibrium interfacial kinetics. An explicit relationship is developed for the mass fluxJ as a function of the characteristic mole ratio of noncondensable gas X, and several simplifications are made to arrive at an effective heat transfer coefficient. A characteristic mole ratio X(c) is also identified that demarcates the transition to a kinetically-limited regime when X << X(c) from a diffusively-limited regime when X >> X(c). Numerical results obtained over a wide range of parameters show that even with a small amount of noncondensable gas, the interfacial temperature drop can be quite significant primarily because of diffusional resistance, an observation that has important practical implications, especially in the field of cryogenic fluid storage. (C) 2009 Elsevier Ltd. All rights reserved. C1 [Kassemi, Mohammad] NASA, Glenn Res Ctr, Natl Ctr Space Explorat Res, Cleveland, OH 44135 USA. [Panzarella, Charles] Equ Engn Grp, Shaker Hts, OH 44122 USA. RP Kassemi, M (reprint author), NASA, Glenn Res Ctr, Natl Ctr Space Explorat Res, 21000 Brookpk Rd,Mailstop 110-3, Cleveland, OH 44135 USA. EM Mohammad.Kassemi@nasa.gov FU Cryogenic Fluid Management (CFM); Exploration Systems Divisions at NASA Headquarters FX This work has been supported by the Cryogenic Fluid Management (CFM) Project at NASA Glenn Research Center through funds provided by the Exploration Systems Divisions at NASA Headquarters. NR 24 TC 9 Z9 9 U1 1 U2 6 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0017-9310 J9 INT J HEAT MASS TRAN JI Int. J. Heat Mass Transf. PD JUL PY 2009 VL 52 IS 15-16 BP 3767 EP 3777 DI 10.1016/j.ijheatmasstransfer.2009.02.027 PG 11 WC Thermodynamics; Engineering, Mechanical; Mechanics SC Thermodynamics; Engineering; Mechanics GA 460FM UT WOS:000267173600037 ER PT J AU Ryan, S Wicklein, M Mouritz, A Riedel, W Schafer, F Thoma, K AF Ryan, S. Wicklein, M. Mouritz, A. Riedel, W. Schaefer, F. Thoma, K. TI Theoretical prediction of dynamic composite material properties for hypervelocity impact simulations SO INTERNATIONAL JOURNAL OF IMPACT ENGINEERING LA English DT Article DE Hypervelocity impact; Orbital debris; Hydrocode; CFRP; Numerical simulation ID DAMAGE PREDICTION; STRENGTH; MODEL AB Recent advances in the description of fibre-reinforced polymer composite material behaviour under extreme loading rates provide a significant extension in capabilities for numerical simulation of hypervelocity impact on composite satellite structures. Given the complexity of the material model, extensive material characterisation is required, however, as the properties of composite materials are commonly tailored for a specific application, experimental characterisation is not efficient, particularly in preliminary design phases. As such, a procedure is outlined in this paper that applies a number of commonly accepted composite mechanics and shock physics theories in conjunction with generalised material properties which allows for the theoretical derivation of a complete material data set for utilisation of the new modelling capabilities. The derivation procedure has been applied to a carbon fibre/epoxy laminate, and is validated through a comparison of derived material properties with experimentally characterised values and numerical simulation or damage induced by hypervelocity impact on a representative space debris shielding configuration employing the CFRP laminate. For the specific structures and impact conditions considered, application of the material property derivation procedure in place of experimental characterisation provided comparable accuracy in the prediction of damage induced by particles impacting at hypervelocity. (c) 2008 Elsevier Ltd. All rights reserved. C1 [Ryan, S.; Wicklein, M.; Riedel, W.; Schaefer, F.; Thoma, K.] FhG Ernst Mach Inst, Fraunhofer Inst High Speed Dynam, Aachen, Germany. [Ryan, S.; Mouritz, A.] RMIT Univ, Sch Aerosp Mech & Mfg Engn, Melbourne, Vic, Australia. RP Ryan, S (reprint author), NASA, Johnson Space Ctr, Mail Code KX,Bldg 267, Houston, TX 77021 USA. EM shannon.j.ryan@nasa.gov OI Schafer, Frank/0000-0001-5719-2259 NR 32 TC 11 Z9 13 U1 4 U2 17 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0734-743X J9 INT J IMPACT ENG JI Int. J. Impact Eng. PD JUL PY 2009 VL 36 IS 7 BP 899 EP 912 DI 10.1016/j.ijimpeng.2008.12.012 PG 14 WC Engineering, Mechanical; Mechanics SC Engineering; Mechanics GA 430FD UT WOS:000264973300003 ER PT J AU Williams, JG Turyshev, SG Boggs, DH AF Williams, James G. Turyshev, Slava G. Boggs, Dale H. TI LUNAR LASER RANGING TESTS OF THE EQUIVALENCE PRINCIPLE WITH THE EARTH AND MOON SO INTERNATIONAL JOURNAL OF MODERN PHYSICS D LA English DT Review DE Lunar laser ranging; equivalence principle; tests of general relativity ID GENERAL-RELATIVITY; DARK-MATTER; MASSIVE BODIES; COSMIC ACCELERATION; EOTVOS EXPERIMENTS; TROJAN ASTEROIDS; GRAVITY-FIELD; SOLAR-SYSTEM; PARAMETERS; PHYSICS AB A primary objective of the lunar laser ranging (LLR) experiment is to provide precise observations of the lunar orbit that contribute to a wide range of science investigations. In particular, time series of the highly accurate measurements of the distance between the Earth and the Moon provide unique information used to determine whether, in accordance with the equivalence principle (EP), these two celestial bodies are falling toward the Sun at the same rate, despite their different masses, compositions, and gravitational self-energies. Thirty-five years since their initiation, analyses of precision laser ranges to the Moon continue to provide increasingly stringent limits on any violation of the EP. Current LLR solutions give (-1.0 +/- 1.4) x 10(-13) for any possible inequality in the ratios of the gravitational and inertial masses for the Earth and Moon, Delta(M-G/M-I). This result, in combination with laboratory experiments on the weak equivalence principle, yields a strong equivalence principle (SEP) test of Delta(M-G/M-I)(SEP) = (-2.0 +/- 2.0) x 10(-13). Such an accurate result allows other tests of gravitational theories. The result of the SEP test translates into a value for the corresponding SEP violation parameter eta of (4.4 +/- 4.5) x 10(-4), where eta = 4 beta - gamma - 3 and both gamma and beta are parametrized post-Newtonian (PPN) parameters. Using the recent result for the parameter gamma derived from the radiometric tracking data from the Cassini mission, the PPN parameter beta (quantifying the nonlinearity of gravitational superposition) is determined to be beta - 1 = (1.2 +/- 1.1) x 10(-4). We also present the history of the LLR effort and describe the technique that is being used. Focusing on the tests of the EP, we discuss the existing data, and characterize the modeling and data analysis techniques. The robustness of the LLR solutions is demonstrated with several different approaches that are presented in the text. We emphasize that near-term improvements in the LLR accuracy will further advance the research on relativistic gravity in the solar system and, most notably, will continue to provide highly accurate tests of the EP. C1 [Williams, James G.; Turyshev, Slava G.; Boggs, Dale H.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Williams, JG (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. FU National Aeronautics and Space Administration FX We thank the staffs of the Observatoire de la Cote d'Azur, Haleakala, and the University of Texas' McDonald ranging stations. The analysis of the planetary data was performed by E. Myles Standish. The research described in this paper was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. NR 113 TC 55 Z9 56 U1 0 U2 5 PU WORLD SCIENTIFIC PUBL CO PTE LTD PI SINGAPORE PA 5 TOH TUCK LINK, SINGAPORE 596224, SINGAPORE SN 0218-2718 EI 1793-6594 J9 INT J MOD PHYS D JI Int. J. Mod. Phys. D PD JUL PY 2009 VL 18 IS 7 BP 1129 EP 1175 PG 47 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 472IJ UT WOS:000268123500007 ER PT J AU Pikuta, EV Hoover, RB Bej, AK Marsic, D Whitman, WB Krader, P AF Pikuta, Elena V. Hoover, Richard B. Bej, Asim K. Marsic, Damien Whitman, William B. Krader, Paul TI Spirochaeta dissipatitropha sp nov., an alkaliphilic, obligately anaerobic bacterium, and emended description of the genus Spirochaeta Ehrenberg 1835 SO INTERNATIONAL JOURNAL OF SYSTEMATIC AND EVOLUTIONARY MICROBIOLOGY LA English DT Article ID AMINO-ACID FERMENTATION; THERMOPHILIC BACTERIUM; FACULTATIVE ANAEROBE; RENATURATION RATES; MARINE SPIROCHETE; OWENS LAKE; CALIFORNIA; DNA AB A novel obligately anaerobic, mesophilic, alkaliphilic spirochaete, strain ASpC2(T), was isolated from an anaerobic sediment of alkaline, hypersaline Owens Lake in California, USA. The Gram-negative cells are motile, helical in shape and 0.23x8.0-18.0 mu m. Growth occurs within the following ranges: 13-41 degrees C, with optimal growth at 35 degrees C; 1-3% (w/v) NaCl, with optimal growth at 2% (w/v) NaCl; and pH 7.8-10.5, with optimal growth at pH 10.0. The novel isolate is strictly alkaliphilic and requires high concentrations of carbonate ions in the medium. It utilizes some sugars, some organic acids, some amino acids, Casamino acids, yeast extract and peptone. The main end products of glucose fermentation are CO(2) and acetate. Strain ASpC2(T) is resistant to kanamycin and rifampicin, but sensitive to ampicillin, chloramphenicol, gentamicin and tetracycline. The DNA G + C content of the new isolate is 43.8 mol%, its genome size is 6x10(8) Da and the melting temperature of its genomic DNA is 71 degrees C. DNA-DNA hybridization experiments demonstrated 46% similarity with the phylogenetically most closely related species, Spirochaeta asiatica Z-7591(T). On the basis of physiological and molecular properties, the new isolate belongs taxonomically to a novel species within the genus Spirochaeta, for which the name Spirochaeta dissipatitropha sp. nov. is proposed (type strain, ASpC2(T)=ATCC BAA-1063(T)=JCM 12856(T)). S. dissipatitropha ASpC2(T) is the second strain in the genus (after Spirochaeta smaragdinae SEBR 4228(T)) that is able to use proteolysis products as the sole energy source, and additional tests have shown that other halo-alkaliphilic spirochaetes (Spirochaeta americana, Spirochaeta alkalica and Spirochaeta africana) are also able to grow on yeast extract alone; therefore, an emended description for the genus Spirochaeta is given. C1 [Pikuta, Elena V.; Hoover, Richard B.] NASA, NSSTC, Astrobiol Lab, Huntsville, AL 35805 USA. [Bej, Asim K.] Univ Alabama, Dept Biol, Birmingham, AL 35294 USA. [Marsic, Damien] Univ Alabama, Struct Biol Lab, Huntsville, AL 35899 USA. [Whitman, William B.] Univ Georgia, Dept Microbiol, Athens, GA 30602 USA. [Krader, Paul] ATCC, Manassas, VA 20110 USA. RP Pikuta, EV (reprint author), NASA, NSSTC, Astrobiol Lab, 320 Sparkman Dr, Huntsville, AL 35805 USA. EM Elena.Pikuta@uah.edu; Richard.Hoover@NASA.GOV RI Marsic, Damien/A-1087-2009 OI Marsic, Damien/0000-0003-0847-8095 NR 28 TC 19 Z9 19 U1 2 U2 8 PU SOC GENERAL MICROBIOLOGY PI READING PA MARLBOROUGH HOUSE, BASINGSTOKE RD, SPENCERS WOODS, READING RG7 1AG, BERKS, ENGLAND SN 1466-5026 J9 INT J SYST EVOL MICR JI Int. J. Syst. Evol. Microbiol. PD JUL PY 2009 VL 59 BP 1798 EP 1804 DI 10.1099/ijs.0.65862-0 PG 7 WC Microbiology SC Microbiology GA 473PM UT WOS:000268219800041 PM 19578151 ER PT J AU Nghiem, SV Balk, D Rodriguez, E Neumann, G Sorichetta, A Small, C Elvidge, CD AF Nghiem, S. V. Balk, D. Rodriguez, E. Neumann, G. Sorichetta, A. Small, C. Elvidge, C. D. TI Observations of urban and suburban environments with global satellite scatterometer data SO ISPRS JOURNAL OF PHOTOGRAMMETRY AND REMOTE SENSING LA English DT Article DE Dense sampling method; Scatterometer; Nighttime lights; Urban; Population ID HUMAN-SETTLEMENTS; CITY LIGHTS; POPULATION; REFLECTANCE; VEGETATION; IMAGERY; CROP; BAND; SAR; MAP AB A global and consistent characterization of land use and land change in urban and suburban environments is crucial for many fundamental social and natural science studies and applications. Presented here is a dense sampling method (DSM) that uses satellite scatterometer data to delineate urban and intraurban areas at a posting scale of about 1 km. DSM results are analyzed together with information on population and housing censuses, with Landsat Enhanced Thematic Mapper Plus (ETM+) imagery, and with Defense Meteorological Satellite Program (DMSP) night-light data. The analyses include Dallas-Fort Worth and Phoenix in the United States, Bogota in Colombia, Dhaka in Bangladesh, Guangzhou in China, and Quito in Ecuador. Results show that scatterometer signatures correspond to buildings and infrastructures in urban and suburban environments. City extents detected by scatterometer data are significantly smaller than city light extents, but not all urban areas are detectable by the current SeaWinds scatterometer on the QuikSCAT satellite. Core commercial and industrial areas with high buildings and large factories are identified as high-backscatter centers. Data from DSM backscatter and DMSP nighttime lights have a good correlation with population density. However, the correlation relations from the two satellite datasets are different for different cities indicating that they contain complementary information. Together with night-light and census data, DSM and satellite scatterometer data provide new observations to study global urban and suburban environments and their changes. Furthermore, the capability of DSM to identify hydrological channels on the Greenland ice sheet and ecological biomes in central Africa demonstrates that DSM can be used to observe persistent structures in natural environments at a km scale, providing contemporaneous data to study human impacts beyond urban and suburban areas. (C) 2009 International Society for Photogrammetry and Remote Sensing, Inc. (ISPRS). Published by Elsevier B.V. All rights reserved. C1 [Nghiem, S. V.; Rodriguez, E.; Neumann, G.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Balk, D.] CUNY, Baruch Coll, Sch Publ Affairs, New York, NY 10010 USA. [Balk, D.] CUNY, Inst Demog Res, New York, NY 10010 USA. [Sorichetta, A.] Univ Milan, Earth Sci Dept Ardito Desio, I-20122 Milan, Italy. [Small, C.] Columbia Univ, Lamont Doherty Earth Observ, New York, NY 10964 USA. [Elvidge, C. D.] NOAA Natl Environm Satellite Data & Informat Serv, Boulder, CO 80305 USA. RP Nghiem, SV (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr,MS 300-235, Pasadena, CA 91109 USA. EM son.v.nghiem@jpl.nasa.gov RI Elvidge, Christopher/C-3012-2009 FU Director's Research and Development Fund (DRDF); NASA Terrestrial Hydrology Program; NASA Cryospheric Sciences Program; NASA Applied Sciences Program FX The research carried out at the Jet Propulsion Laboratory (JPL), California Institute of Technology, was supported under a contract with the National Aeronautics and Space Administration (NASA) and funded through the Director's Research and Development Fund (DRDF) program. The original development of the SSSP infrastructure at JPL was supported by the NASA Terrestrial Hydrology Program. The research related to the Greenland ice sheet at JPL was supported by the NASA Cryospheric Sciences Program. The research related to drought and vegetation change at JPL was supported by the NASA Applied Sciences Program. Coauthors Balk and Sorichetta were affiliated with the Columbia University's Center for international Earth Science Information Network (CIESIN) when this study began. We thank the CIESIN's Socioeconomic Data and Application Center for support in the preliminary work leading to this study. The research carried out at the City University of New York, the Columbia University, and the University of Milan was also supported by the DRDF program. We thank Peggy Li of JPL for the overlay of the DSM image on the Principe Island. NR 44 TC 14 Z9 15 U1 7 U2 38 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 JUL PY 2009 VL 64 IS 4 BP 367 EP 380 DI 10.1016/j.isprsjprs.2009.01.004 PG 14 WC Geography, Physical; Geosciences, Multidisciplinary; Remote Sensing; Imaging Science & Photographic Technology SC Physical Geography; Geology; Remote Sensing; Imaging Science & Photographic Technology GA 479HL UT WOS:000268650200004 ER PT J AU Kanki, BC Rogers, DG Bessone, L Parke, B Sandal, GM Whiteley, I AF Kanki, Barbara C. Rogers, David G. Bessone, Loredana Parke, Bonny Sandal, Gro M. Whiteley, Iya TI TEAM PERFORMANCE AND SPACE SAFETY SO JBIS-JOURNAL OF THE BRITISH INTERPLANETARY SOCIETY LA English DT Article DE Team performance; human factors; human communications; organizational factors; team training ID SHUTTLE/MIR; STATION; ISSUES AB This paper discusses how space safety is influenced by the ability of teams to work and communicate effectively together. A multi-national team of six authors provides different perspectives on human systems, from both research and operational points of view. When operations involve teams whose members cross organizational and cultural boundaries as they do ill current space operations, it is especially critical and challenging to facilitate the most effective team performance. Three key factors that affect team performance and space safety are discussed: (1) communication as related to team performance; (2) the influence of organizations, teams and culture and (3) team training interventions. Relevant research and current practices are described for each of the three areas and a summary in the form of recommendations is provided. C1 [Kanki, Barbara C.; Parke, Bonny] NASA, Ames Res Ctr, SJSUF, Moffett Field, CA 94035 USA. [Rogers, David G.] Sci Applicat Int Corp, Houston, TX 77058 USA. [Bessone, Loredana] European Space Agcy, European Astronaut Ctr, D-51143 Cologne, Germany. [Sandal, Gro M.] Univ Bergen, Dept Psychosocial Sci, N-5015 Bergen, Norway. [Whiteley, Iya] European Space Agcy, European Astronaut Ctr, D-51147 Cologne, Germany. RP Kanki, BC (reprint author), NASA, Ames Res Ctr, SJSUF, M-S 262-4, Moffett Field, CA 94035 USA. EM barbara.g.kanki@nasa.gov; david.g.rogers@nasa.gov; loredana.bessone@esa.int; bonny.parke@nasa.gov; gro.sandal@psysp.uib.no; iya.whiteley@vega.de NR 41 TC 1 Z9 1 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 JUL-AUG PY 2009 VL 62 IS 7-8 BP 273 EP 281 PG 9 WC Engineering, Aerospace; Astronomy & Astrophysics; Geosciences, Multidisciplinary SC Engineering; Astronomy & Astrophysics; Geology GA 532XR UT WOS:000272784200007 ER PT J AU Goldberg, RK Binienda, WK AF Goldberg, Robert K. Binienda, Wieslaw K. TI Ballistic Impact and Crashworthiness Response of Aerospace Structures SO JOURNAL OF AEROSPACE ENGINEERING LA English DT Editorial Material C1 [Goldberg, Robert K.] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. [Binienda, Wieslaw K.] Univ Akron, Dept Civil Engn, Akron, OH 44325 USA. RP Goldberg, RK (reprint author), NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. EM Robert.K.Goldberg@nasa.gov; wbinienda@uakron.edu NR 0 TC 0 Z9 0 U1 2 U2 3 PU ASCE-AMER SOC CIVIL ENGINEERS PI RESTON PA 1801 ALEXANDER BELL DR, RESTON, VA 20191-4400 USA SN 0893-1321 J9 J AEROSPACE ENG JI J. Aerosp. Eng. PD JUL PY 2009 VL 22 IS 3 BP 199 EP 200 DI 10.1061/(ASCE)0893-1321(2009)22:3(199) PG 2 WC Engineering, Aerospace; Engineering, Civil SC Engineering GA 458VF UT WOS:000267053100001 ER PT J AU Fasanella, EL AF Fasanella, Edwin L. TI Multiterrain Earth Landing Systems Applicable for Manned Space Capsules SO JOURNAL OF AEROSPACE ENGINEERING LA English DT Article AB A key element of the President's Vision for Space Exploration is the development of a new space transportation system to replace Shuttle that will enable manned exploration of the moon, Mars, and beyond. The National Aeronautics and Space Administration has created the Constellation Program to develop this architecture, which includes the Ares launch vehicle and Orion manned spacecraft. The Orion spacecraft must carry six astronauts and its primary structure should be reusable, if practical. These requirements led the Constellation Program to consider a baseline land landing on return to earth. To assess the landing system options for Orion, a review of current operational parachute landing systems such as those used for the F-111 escape module and the Soyuz is performed. In particular, landing systems with airbags and retrorockets that would enable reusability of the Orion capsule are investigated. In addition, Apollo tests and analyses conducted in the 1960s for both water and land landings are reviewed. Finally, test data and dynamic finite-element simulations are presented to understand land landings for the Orion spacecraft. C1 NASA, Struct Dynam Branch, Langley Res Ctr, Hampton, VA 23681 USA. RP Fasanella, EL (reprint author), NASA, Struct Dynam Branch, Langley Res Ctr, 12 W Bush Rd, Hampton, VA 23681 USA. EM edwin.l.fasanella@nasa.gov NR 22 TC 3 Z9 3 U1 0 U2 3 PU ASCE-AMER SOC CIVIL ENGINEERS PI RESTON PA 1801 ALEXANDER BELL DR, RESTON, VA 20191-4400 USA SN 0893-1321 J9 J AEROSPACE ENG JI J. Aerosp. Eng. PD JUL PY 2009 VL 22 IS 3 BP 201 EP 213 DI 10.1061/(ASCE)0893-1321(2009)22:3(201) PG 13 WC Engineering, Aerospace; Engineering, Civil SC Engineering GA 458VF UT WOS:000267053100002 ER PT J AU Lawrence, C Littell, JD Fasanella, EL Tabiei, A AF Lawrence, Charles Littell, Justin D. Fasanella, Edwin L. Tabiei, Ala TI Orion Crew Member Injury Predictions during Land and Water Landings SO JOURNAL OF AEROSPACE ENGINEERING LA English DT Article AB A review of astronaut whole body impact tolerance is discussed for land or water landings of the next generation manned space capsule named Orion. LS-DYNA simulations of Orion capsule landings are performed to produce a low, moderate, and high probability of injury. The paper evaluates finite-element (FE) seat and occupant simulations for assessing injury risk for the Orion crew and compares these simulations to whole body injury models commonly referred to as the Brinkley criteria. The FE seat and crash dummy models allow for varying the occupant restraint systems, cushion materials, side constraints, flailing of limbs, and detailed seat/occupant interactions to minimize landing injuries to the crew. The FE crash test dummies used in conjunction with the Brinkley criteria provides a useful set of tools for predicting potential crew injuries during vehicle landings. C1 [Lawrence, Charles] NASA, Glenn Res Ctr, Cleveland, OH USA. [Littell, Justin D.] Univ Akron, Akron, OH 44325 USA. [Fasanella, Edwin L.] NASA, Langley Res Ctr, Hampton, VA 23665 USA. [Tabiei, Ala] Multiphys Simulat Engn, Mason, OH USA. RP Lawrence, C (reprint author), NASA, Glenn Res Ctr, Cleveland, OH USA. EM lawrence@nasa.gov; justin.d.littell@grc.nasa.gov; fasanella@nasa.gov; atabiei@aol.com NR 13 TC 1 Z9 2 U1 0 U2 7 PU ASCE-AMER SOC CIVIL ENGINEERS PI RESTON PA 1801 ALEXANDER BELL DR, RESTON, VA 20191-4400 USA SN 0893-1321 J9 J AEROSPACE ENG JI J. Aerosp. Eng. PD JUL PY 2009 VL 22 IS 3 BP 214 EP 221 DI 10.1061/(ASCE)0893-1321(2009)22:3(214) PG 8 WC Engineering, Aerospace; Engineering, Civil SC Engineering GA 458VF UT WOS:000267053100003 ER PT J AU Firko, JL Albert, JJ Lee, TJ Boyer, AM Gabrys, JW Carney, KS AF Firko, Jason L. Albert, Jeremie J. Lee, Timothy J. Boyer, Alexander M. Gabrys, Jonathan W. Carney, Kelly S. TI Shuttle Debris Impact Analysis: Postreturn to Flight Real-Time Mission Support SO JOURNAL OF AEROSPACE ENGINEERING LA English DT Article AB Prior to the Columbia accident, quantitative impact assessment tools were not available to analyze debris impacts onto the Shuttle's thermal protection system. Following the accident, the Columbia Accident Investigation Board recommended changes to increase the safety of future shuttle flights; one component was the development of physics-based analytical capabilities to evaluate damage due to debris impacts. This paper will present an overview of real time debris assessment impact analysis conducted by the Boeing Philadelphia Advanced Structural Analysis Impact Analysis Team in support of Space Shuttle missions since Return to Flight, the first mission after the Columbia accident. Specifically, analyses performed in support of missions STS-114, 121 and 117 will be presented. For each of these cases, an overview of the structural and material model development will be provided, and results of each analysis will be presented followed by a discussion of how the results lead into real time mission decisions. This work illustrates the importance of maintaining a physics-based real-time analysis capability as a vital instrument in supporting the safety of future spaceflight missions. C1 [Firko, Jason L.; Albert, Jeremie J.; Lee, Timothy J.; Boyer, Alexander M.; Gabrys, Jonathan W.] Boeing Co, Philadelphia, PA 19142 USA. [Carney, Kelly S.] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. RP Firko, JL (reprint author), Boeing Co, POB 16858,MC P24-25, Philadelphia, PA 19142 USA. EM jason.l.firko@boeing.com NR 4 TC 0 Z9 0 U1 1 U2 1 PU ASCE-AMER SOC CIVIL ENGINEERS PI RESTON PA 1801 ALEXANDER BELL DR, RESTON, VA 20191-4400 USA SN 0893-1321 J9 J AEROSPACE ENG JI J. Aerosp. Eng. PD JUL PY 2009 VL 22 IS 3 BP 222 EP 228 DI 10.1061/(ASCE)0893-1321(2009)22:3(222) PG 7 WC Engineering, Aerospace; Engineering, Civil SC Engineering GA 458VF UT WOS:000267053100004 ER PT J AU Jackson, KE Fuchs, YT Kellas, S AF Jackson, Karen E. Fuchs, Yvonne T. Kellas, Sotiris TI Overview of the National Aeronautics and Space Administration Subsonic Rotary Wing Aeronautics Research Program in Rotorcraft Crashworthiness SO JOURNAL OF AEROSPACE ENGINEERING LA English DT Article ID SIMULATION AB This paper provides an overview of rotorcraft crashworthiness research being conducted at the National Aeronautics and Space Administration Langley Research Center under sponsorship of the Subsonic Rotary Wing aeronautics program. The research is focused in two areas: development of an externally deployable energy attenuating concept and improved prediction of rotorcraft crashworthiness. The deployable energy absorber (DEA) is a composite honeycomb structure, with a unique flexible hinge design that allows the honeycomb to be packaged and remain flat until needed for deployment. The capabilities of the DEA have been demonstrated through component crush tests and vertical drop tests of a retrofitted fuselage section onto different surfaces or terrain. The research on improved prediction of rotorcraft crashworthiness is focused in several areas including simulating occupant responses and injury risk assessment, predicting multiterrain impact, and utilizing probabilistic analysis methods. A final task is to perform a system-integrated simulation of a full-scale helicopter crash test onto a rigid surface. A brief description of each research task is provided along with a summary of recent accomplishments. C1 [Jackson, Karen E.; Fuchs, Yvonne T.; Kellas, Sotiris] NASA, Langley Res Ctr, Hampton, VA 23681 USA. RP Jackson, KE (reprint author), NASA, Langley Res Ctr, MS 495,12 W Bush Rd, Hampton, VA 23681 USA. EM karen.e.jackson-1@nasa.gov; yvonne.t.fachs@nasa.gov; sotiris.kellas@nasa.gov NR 17 TC 10 Z9 10 U1 0 U2 5 PU ASCE-AMER SOC CIVIL ENGINEERS PI RESTON PA 1801 ALEXANDER BELL DR, RESTON, VA 20191-4400 USA SN 0893-1321 J9 J AEROSPACE ENG JI J. Aerosp. Eng. PD JUL PY 2009 VL 22 IS 3 BP 229 EP 239 DI 10.1061/(ASCE)0893-1321(2009)22:3(229) PG 11 WC Engineering, Aerospace; Engineering, Civil SC Engineering GA 458VF UT WOS:000267053100005 ER PT J AU Pereira, JM Revilock, DM AF Pereira, J. Michael Revilock, Duane M., Jr. TI Ballistic Impact Response of Kevlar 49 and Zylon under Conditions Representing Jet Engine Fan Containment SO JOURNAL OF AEROSPACE ENGINEERING LA English DT Article ID SIMULATION; MODEL; ARMOR AB A ballistic impact test program was conducted to provide validation data for the development of numerical models of blade out events in fabric containment systems. The impact response of two different fiber materials-Kevlar 49 (E.I. DuPont Nemours and Company) and Zylon AS (Toyobo Co., Ltd.) was studied by firing metal projectiles into dry woven fabric specimens using a gas gun. The shape, mass, orientation, and velocity of the projectile were varied and recorded. In most cases the tests were designed such that the projectile would perforate the specimen, allowing measurement of the energy absorbed by the fabric. The results for both Zylon and Kevlar presented here represent a useful set of data for the purposes of establishing and validating numerical models for predicting the response of fabrics under conditions simulating those of a jet engine blade release situation. In addition some useful empirical observations were made regarding the effects of projectile orientation and the relative performance of the different materials. C1 [Pereira, J. Michael; Revilock, Duane M., Jr.] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. RP Pereira, JM (reprint author), NASA, Glenn Res Ctr, 21000 Brookpk Rd, Cleveland, OH 44135 USA. EM mike.pereira@nasa.gov; duane.m.revilock@grc.nasa.gov FU Federal Aviaion Administration's Aircraft Catastrophic Failure Prevention Research Program FX The writers wish to thank William Emmerling and Donald Altobelli of the Federal Aviaion Administration's Aircraft Catastrophic Failure Prevention Research Program for their support and guidance. Materials tested in this effort were provided by the FAA. NR 16 TC 9 Z9 11 U1 0 U2 2 PU ASCE-AMER SOC CIVIL ENGINEERS PI RESTON PA 1801 ALEXANDER BELL DR, RESTON, VA 20191-4400 USA SN 0893-1321 J9 J AEROSPACE ENG JI J. Aerosp. Eng. PD JUL PY 2009 VL 22 IS 3 BP 240 EP 248 DI 10.1061/(ASCE)0893-1321(2009)22:3(240) PG 9 WC Engineering, Aerospace; Engineering, Civil SC Engineering GA 458VF UT WOS:000267053100006 ER PT J AU Littell, JD Binienda, WK Roberts, GD Goldberg, RK AF Littell, Justin D. Binienda, Wieslaw K. Roberts, Gary D. Goldberg, Robert K. TI Characterization of Damage in Triaxial Braided Composites under Tensile Loading SO JOURNAL OF AEROSPACE ENGINEERING LA English DT Article ID TEXTILE COMPOSITES AB Carbon fiber composites that utilize flattened, large tow yarns in woven or braided forms are being used in many aerospace applications. The complex fiber architecture and large unit cell size in these materials present challenges for both understanding the deformation process and measuring reliable material properties. In this paper composites made using flattened 12k and 24k (referring to the number of fibers in the fiber tow) standard modulus carbon fiber yarns in a 0 degrees/+60 degrees/-60 degrees triaxial braided architecture are examined. Standard straight-sided tensile coupons were tested with the 0 degrees axial braid fibers either parallel to (axial tensile test) or perpendicular to (transverse tensile test) the applied tensile load. The nonuniform surface strain resulting from the triaxial braided architecture was examined using photogrammetry. Local regions of high strain concentration were examined to identify where failure initiates and to determine the local strain at the time of failure initiation. Splitting within fiber bundles was the first failure mode observed at low to intermediate strains. For axial tensile tests the splitting was primarily in the +/- 60 degrees bias fibers, which were oriented 60 degrees to the applied load. At higher strains in the axial tensile test, out-of-plane deformation associated with localized delamination between fiber bundles or damage within fiber bundles was observed. For transverse tensile tests, the splitting was primarily in the 0 degrees axial fibers, which were oriented transverse to the applied load. The initiation and accumulation of local damage caused the global transverse stress-strain curves to become nonlinear and caused failure to occur at a reduced ultimate strain for both the axial and transverse tensile tests. Extensive delamination at the specimen edges was also observed. Modifications to the standard straight-sided coupon geometry are needed to minimize these edge effects when testing the large unit cell type of material examined in this work. C1 [Littell, Justin D.; Binienda, Wieslaw K.] Univ Akron, Akron, OH 44325 USA. [Roberts, Gary D.; Goldberg, Robert K.] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. RP Littell, JD (reprint author), Univ Akron, 302 Buchtel Mall, Akron, OH 44325 USA. EM justin.d.littell@nasa.gov; wbinienda@uakron.edu; gary.d.roberts@nasa.gov; Robert.K.Goldberg@nasa.gov NR 19 TC 20 Z9 20 U1 0 U2 5 PU ASCE-AMER SOC CIVIL ENGINEERS PI RESTON PA 1801 ALEXANDER BELL DR, RESTON, VA 20191-4400 USA SN 0893-1321 J9 J AEROSPACE ENG JI J. Aerosp. Eng. PD JUL PY 2009 VL 22 IS 3 BP 270 EP 279 DI 10.1061/(ASCE)0893-1321(2009)22:3(270) PG 10 WC Engineering, Aerospace; Engineering, Civil SC Engineering GA 458VF UT WOS:000267053100009 ER PT J AU Carney, KS DuBois, PA Buyuk, M Kan, S AF Carney, Kelly S. DuBois, Paul A. Buyuk, Murat Kan, Steve TI Generalized, Three-Dimensional Definition, Description, and Derived Limits of the Triaxial Failure of Metals SO JOURNAL OF AEROSPACE ENGINEERING LA English DT Article ID DUCTILE FRACTURE; GROWTH; VOIDS AB Metal failure in many applications, such as ballistic impact, containment, shielding, metal forming, and crashworthiness, occurs while the material is in a three-dimensional state of stress. Many previous definitions of triaxiality use two invariants to define the relative stress state in a virtual element, leading to a characterization that can be better thought of as biaxial. In this paper, an additional parameter based upon the third stress invariant is defined, which extends the characterization of the state of stress to three dimensions and to true triaxiality. The relation of the two parameters is explored and limits are found in the failure surface, which is used in defining the critical failure regions. Standard tests are examined to determine if they can provide enough data to construct these regions of interest and new tests are proposed, which envelope the limits and thus define this failure surface. C1 [Carney, Kelly S.] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. [Buyuk, Murat; Kan, Steve] George Washington Univ, FHwA NHTSA Natl Crash Anal Ctr, Ashburn, VA 20147 USA. RP Carney, KS (reprint author), NASA, Glenn Res Ctr, 21000 Brookpk Rd, Cleveland, OH 44135 USA. EM kelly.s.carney@nasa.gov FU Federal Aviation Administration's Aircraft Catastrophic Failure Prevention Research Program; Hughes Technical Center, Atlantic City, N.J. FX The writers wish to thank William Emmerling and Donald Altobelli of the Federal Aviation Administration's Aircraft Catastrophic Failure Prevention Research Program, and Hughes Technical Center, Atlantic City, N.J., for their support and guidance. The efforts of Paul DuBois, Murat Buyuk, and Steve Kan were funded by a Federal Aviation Administration grant to the National Crash Analysis Center, George Washington University, Washington, D.C. NR 9 TC 1 Z9 1 U1 0 U2 1 PU ASCE-AMER SOC CIVIL ENGINEERS PI RESTON PA 1801 ALEXANDER BELL DR, RESTON, VA 20191-4400 USA SN 0893-1321 J9 J AEROSPACE ENG JI J. Aerosp. Eng. PD JUL PY 2009 VL 22 IS 3 BP 280 EP 286 DI 10.1061/(ASCE)0893-1321(2009)22:3(280) PG 7 WC Engineering, Aerospace; Engineering, Civil SC Engineering GA 458VF UT WOS:000267053100010 ER PT J AU Edwards, JW Spain, CV Keller, DF Moses, RW Schuster, DM AF Edwards, John W. Spain, Charles V. Keller, Donald F. Moses, Robert W. Schuster, David M. TI Transport Wing Flutter Model Transonic Limit Cycle Oscillation Test SO JOURNAL OF AIRCRAFT LA English DT Article ID FIGHTER AB The model for aeroelastic validation research involving computation semispan wind-tunnel model, a transport wing-fuselage flutter model, was tested in NASA Langley's Transonic Dynamics Tunnel with the goal of obtaining experimental limit cycle oscillation behavior data at transonic separation onset conditions. This research model is notable for its inexpensive construction and instrumentation installation procedures. Unsteady pressures and wing responses were obtained for three wing-tip configurations: clean, tip store, and winglet. Traditional flutter boundaries were measured over the range of M = 0.64.9, and maps of limit cycle oscillation behavior were made in the range of M = 0.85-0.95. The effects of dynamic pressure and angle of attack were measured. Testing in both R134a heavy gas and air provided unique data on the Reynolds number, transition effects, and the effect of speed of sound on limit cycle oscillation behavior. This report gives an overview of the test results, including experimental flutter boundaries, and the conditions involving shock-induced transonic How separation onset at low wing angles, including maps of limit cycle oscillation behavior. C1 [Edwards, John W.; Spain, Charles V.; Keller, Donald F.] NASA, Langley Res Ctr, Aeroelast Branch, Hampton, VA 23681 USA. [Moses, Robert W.] NASA, Langley Res Ctr, Atmospher Flight & Entry Syst Branch, Hampton, VA 23681 USA. NR 21 TC 3 Z9 3 U1 0 U2 6 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 JUL-AUG PY 2009 VL 46 IS 4 BP 1104 EP 1113 DI 10.2514/1.30079 PG 10 WC Engineering, Aerospace SC Engineering GA 482RJ UT WOS:000268906100003 ER PT J AU Coppenbarger, RA Mead, RW Sweet, DN AF Coppenbarger, Richard A. Mead, Rob W. Sweet, Douglas N. TI Field Evaluation of the Tailored Arrivals Concept for Datalink-Enabled Continuous Descent Approach SO JOURNAL OF AIRCRAFT LA English DT Article; Proceedings Paper CT AIAA 7th Aviation Technology, Integration and Operations Conference/2nd CEIAT International Conference on Innovation and Integration in Aerospace Sciences/17th LTA Systems Technology Conference CY SEP 18-20, 2007 CL Belfast, NORTH IRELAND SP Amer Inst Aeronaut & Astronaut, Ctr Excellence Integrated Aircraft Technologies AB Allowing aircraft to descend uninterrupted at low engine power, continuous descent operations promise to maximize fuel efficiency while minimizing environmental impact. Tailored arrivals is a concept for enabling continuous descents under constrained airspace conditions by integrating advanced air and ground automation through digital datalink. Operational trials were completed in January 2007 involving transpacific flights into San Francisco during early morning hours. Leveraging newly deployed Federal Aviation Administration automation in the oceanic environment, trajectory-based clearances were transmitted by datalink to Boeing 777 aircraft equipped with future air navigation system avionics. NASA's prototype ground-based automation for high-density arrival management tailored trajectory clearances to accommodate artificially imposed metering constraints. Upon sharing wind and descent-speed-intent data, ground-based and airborne automation were found to predict meter-fix arrival times to within a mean accuracy of 3 s over a 25 min prediction horizon. Corresponding mean altitude and along-track prediction errors of ground-based automation were -500 ft and -1.3 n mile, respectively, in comparison with surveillance truth. A benefits analysis suggests Boeing 777 fuel savings of between 200 and 3000 lb per flight (depending highly upon baseline traffic conditions) together with a corresponding reduction in CO(2) emissions of between 700 and 10,000 lb per flight. C1 [Coppenbarger, Richard A.] NASA, Ames Res Ctr, Automat Concepts Res Branch, Moffett Field, CA 94043 USA. [Mead, Rob W.] Boeing Co, Air Ground Commun & Tailored Arrivals, Boeing Phantom Works Adv Air Traff Management, Chicago, IL 60606 USA. [Sweet, Douglas N.] Sensis Corp, Sensis Seagull Technol Ctr, Campbell, CA 95008 USA. RP Coppenbarger, RA (reprint author), NASA, Ames Res Ctr, Automat Concepts Res Branch, Mail Stop 210-10, Moffett Field, CA 94043 USA. NR 14 TC 12 Z9 12 U1 0 U2 9 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 JUL-AUG PY 2009 VL 46 IS 4 BP 1200 EP 1209 DI 10.2514/1.39795 PG 10 WC Engineering, Aerospace SC Engineering GA 482RJ UT WOS:000268906100012 ER PT J AU Yeo, H Johnson, W AF Yeo, Hyeonsoo Johnson, Wayne TI Optimum Design of a Compound Helicopter SO JOURNAL OF AIRCRAFT LA English DT Article ID COMPREHENSIVE ANALYSIS; ROTORS AB A design and aeromechanics investigation was conducted for a 100,000 lb compound helicopter with a single main rotor that will cruise at a condition of 250 kt at 4000 ft/95 degrees F. Performance, stability, and control analyses were conducted with the comprehensive rotorcraft analysis CAMRAD II. Wind-tunnel test measurements of the performance of the H-34 and UH-1D rotors at high advance ratios were compared with calculations to assess the accuracy of the analysis for the design of a high-speed helicopter. In general, good correlation was obtained with the test data. An assessment of various design parameters (disk loading, blade loading, wing loading) on the performance of the compound helicopter was made. Lower wing loading (larger wing area) and higher design blade loading (smaller blade chord) increased the aircraft lift-to-drag ratio. However, disk loading has a small influence on the aircraft lift-to-drag ratio. A rotor parametric study showed that most of the benefit of slowing the rotor occurred at the initial 20-30% reduction of the advancing blade tip Mach number. No stability issues were observed with the current design, and the control derivatives did not change much with speed, but did exhibit significant coupling. C1 [Johnson, Wayne] NASA, Ames Res Ctr, Flight Vehicle Res & Technol Div, Moffett Field, CA 94035 USA. EM hyeonsoo.yeo@us.army.mil NR 10 TC 14 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 0021-8669 J9 J AIRCRAFT JI J. Aircr. PD JUL-AUG PY 2009 VL 46 IS 4 BP 1210 EP 1221 DI 10.2514/1.40101 PG 12 WC Engineering, Aerospace SC Engineering GA 482RJ UT WOS:000268906100013 ER PT J AU Yeo, H Johnson, W AF Yeo, Hyeonsoo Johnson, Wayne TI Performance and Design Investigation of Heavy Lift Tilt-Rotor with Aerodynamic Interference Effects SO JOURNAL OF AIRCRAFT LA English DT Article AB Performance calculations were conducted for 146,600 lb conventional and quad tilt-rotors, which are to cruise at 300 kt at a 4000 ft/95 degrees F condition. Aerodynamic interference effects on the aircraft cruise performance were quantified. Aerodynamic interference improves the aircraft lift-to-drag ratio of the baseline conventional tilt-rotor. However, interference degrades the aircraft performance of the baseline quad tilt-rotor, mostly due to the unfavorable effect,; from the front wing to the rear wing. A parametric study was conducted to understand the effects of design parameters on the performance of the aircraft. A reduction in rotor tip speed increased the aircraft lift-to-drag ratio the most among the design parameters investigated. C1 [Johnson, Wayne] NASA, Ames Res Ctr, Aeromech Branch, Moffett Field, CA 94035 USA. EM hyeonsoo.yeo@us.army.mil NR 15 TC 13 Z9 15 U1 1 U2 7 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 JUL-AUG PY 2009 VL 46 IS 4 BP 1231 EP 1239 DI 10.2514/1.40102 PG 9 WC Engineering, Aerospace SC Engineering GA 482RJ UT WOS:000268906100015 ER PT J AU Sutliff, DL Jones, MG AF Sutliff, Daniel L. Jones, Michael G. TI Low-Speed Fan Noise Attenuation from a Foam-Metal Liner SO JOURNAL OF AIRCRAFT LA English DT Article; Proceedings Paper CT AIAA/CEAS 14th Aeroacoustics Conference CY MAY 05-JUL 05, 2008 CL Vancouver, CANADA SP AIAA, CEAS ID ACOUSTIC PROPERTIES AB A foam-metal liner for attenuation of fan noise was developed for and tested on a low-speed fan. This type of liner represents a significant advance over traditional liners, due to the possibility of placement in close proximity to the rotor. An advantage of placing treatment in this region is that the acoustic near field is modified, thereby inhibiting the noise-generation mechanism. This can result in higher attenuation levels than could be achieved by liners located in the nacelle inlet. In addition, foam-metal liners could potentially replace the fan rub strip and containment components, ultimately reducing engine components and thus weight, which can result in a systematic increase in noise reduction and engine performance. Foam-metal liners have the potential to reduce fan noise by 4 dB based on this study. C1 [Sutliff, Daniel L.] NASA, John H Glenn Res Ctr Lewis Field, Acoust Branch, Cleveland, OH 44135 USA. [Jones, Michael G.] NASA, Langley Res Ctr Res, Res & Technol Directorate, Struct Acoust Branch, Hampton, VA 23681 USA. RP Sutliff, DL (reprint author), NASA, John H Glenn Res Ctr Lewis Field, Acoust Branch, Mail Stop 54-3, Cleveland, OH 44135 USA. NR 9 TC 6 Z9 6 U1 1 U2 3 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 JUL-AUG PY 2009 VL 46 IS 4 BP 1381 EP 1394 DI 10.2514/1.41369 PG 14 WC Engineering, Aerospace SC Engineering GA 482RJ UT WOS:000268906100030 ER PT J AU Przekop, A Rizzi, SA AF Przekop, Adam Rizzi, Stephen A. TI Nonlinear Reduced-Order Analysis with Time-Varying Spatial Loading Distributions SO JOURNAL OF AIRCRAFT LA English DT Article; Proceedings Paper CT AIAA/ASME/ASCE/AHS/ASC 49th Structures Structural Dynamic, and Materials Conference CY APR 07-10, 2008 CL Schaumburg, IL SP AIAA, ASME, ASCE, AHS, ASC AB Oscillating shocks acting in combination with high-intensity acoustic loadings present a challenge to the design of resilient hypersonic-flight vehicle structures. This paper addresses some features of this loading condition and certain aspects of a nonlinear reduced-order analysis with emphasis on system identification, leading to the formation of a robust modal basis. The nonlinear dynamic response of a composite structure subject to the simultaneous action of locally strong oscillating pressure gradients and high-intensity acoustic loadings is considered. The reduced-order analysis used in this work has been previously demonstrated to be both computationally efficient and accurate for time-invariant spatial loading distributions, provided that an appropriate modal basis is used. The challenge of the present study is to identify a suitable basis for loadings with time-varying spatial distributions. Using a proper orthogonal decomposition and modal expansion, it is shown that such a basis can be developed. The basis is made more robust by incrementally expanding it to account for changes in the location, frequency, and span of the oscillating pressure gradient. C1 [Przekop, Adam] Analyt Serv & Mat Inc, Hampton, VA 23666 USA. [Rizzi, Stephen A.] NASA, Langley Res Ctr, Struct Acoust Branch, Hampton, VA 23681 USA. RP Przekop, A (reprint author), Analyt Serv & Mat Inc, Hampton, VA 23666 USA. NR 15 TC 6 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 0021-8669 J9 J AIRCRAFT JI J. Aircr. PD JUL-AUG PY 2009 VL 46 IS 4 BP 1395 EP 1402 DI 10.2514/1.39790 PG 8 WC Engineering, Aerospace SC Engineering GA 482RJ UT WOS:000268906100031 ER PT J AU Makeev, MA Sundaresh, S Srivastava, D AF Makeev, Maxim A. Sundaresh, Suman Srivastava, Deepak TI Shock-wave propagation through pristine a-SiC and carbon-nanotube-reinforced a-SiC matrix composites SO JOURNAL OF APPLIED PHYSICS LA English DT Article DE amorphous semiconductors; carbon nanotubes; molecular dynamics method; particle reinforced composites; shock waves; silicon compounds ID MOLECULAR-DYNAMICS SIMULATIONS; FINITE-TEMPERATURE PROPERTIES; ATOMISTIC SIMULATION; PHASE-TRANSITIONS; HIGH-PRESSURE; COMPRESSION; AMORPHIZATION; LATTICE; SOLIDS; FRONT AB We report on the results of a large-scale molecular dynamics simulation study of shock-wave propagation in pristine amorphous silicon carbide and carbon-nanotube-reinforced amorphous silicon carbide matrix composites. We seek to understand the effects of ensembles of aligned nanotubes, both transversely and longitudinally oriented, on the shock-wave structure and dynamics and structural rearrangements taking place in the shock-loaded composite materials. It is found that the presence of aligned nanotubes in amorphous silicon carbide matrix leads to a reduction of shock-wave velocity and modifies the shock-wave front structure in a wide range of impact velocities. The temporal evolution of density profiles behind the shock-wave front is studied and conclusions are drawn regarding the effects of carbon nanotubes on the structural rearrangements in the shock-loaded composite materials. The mechanisms of carbon nanotube failure under shock loadings and their implications for energy dissipation rates in composite material systems are discussed for both considered cases of carbon nanotube alignments. C1 [Makeev, Maxim A.; Sundaresh, Suman; Srivastava, Deepak] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Makeev, MA (reprint author), NASA, Ames Res Ctr, Mail Stop 229-1, Moffett Field, CA 94035 USA. EM Maxim.A.Makeev@nasa.gov; ssundaresh@cornell.edu; deepak.srivastava-1@nasa.gov FU NASA [NAS2-03144] FX D. S. and M. A. M. gratefully acknowledge support from NASA (Contract No. NAS2-03144 to UARC). NR 51 TC 5 Z9 5 U1 6 U2 25 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 JUL 1 PY 2009 VL 106 IS 1 AR 014311 DI 10.1063/1.3152587 PG 8 WC Physics, Applied SC Physics GA 471NK UT WOS:000268065000112 ER PT J AU Sehirlioglu, A Sayir, A Dynys, F AF Sehirlioglu, Alp Sayir, Ali Dynys, Fred TI High temperature properties of BiScO3-PbTiO3 piezoelectric ceramics SO JOURNAL OF APPLIED PHYSICS LA English DT Article DE aerospace components; aerospace materials; bismuth compounds; dielectric hysteresis; dielectric losses; electrical conductivity; electromechanical effects; ferroelectric ceramics; ferroelectric Curie temperature; high field effects; high-temperature effects; lead compounds; piezoceramics; piezoelectricity; sintering ID SOLID-SOLUTION AB Smart actuators and intelligent structures are sought after for aeronautical applications. As a result of high Curie temperature (430 degrees C) and piezoelectric coefficient (>200 pC/N), BiScO3-PbTiO3 (BS-PT) ceramics are prospective materials for high temperature actuators. This paper reports on the temperature dependent electrical, ferroelectric, and electromechanical properties of liquid phase sintered BS-PT ceramics. Compared to solid state sintered BS-PT, liquid phase sintered BS-PT with Bi2O3 showed improved electrical performance: (1) threefold reduction in loss tangent at elevated temperatures, (2) fivefold increase in dc resistivity at high electrical fields, and (3) 15% increase in high field piezoelectric coefficient. Hysteresis loops of the highly resistive ceramics were saturated and showed no major dependence on the magnitude and the frequency of the applied field. BS-PT ceramics exhibit depoling behavior at temperatures below (>350 degrees C) the Curie temperature (430 degrees C). Liquid phase sintering using excess Bi2O3 is shown to be a promising approach to produce superior BS-PT ceramics for high temperature actuators. C1 [Sehirlioglu, Alp; Sayir, Ali; Dynys, Fred] NASA, John Glenn Res Ctr, Cleveland, OH 44135 USA. [Sehirlioglu, Alp; Sayir, Ali] Case Western Reserve Univ, Dept Mat Sci & Engn, Cleveland, OH 44106 USA. RP Sehirlioglu, A (reprint author), NASA, John Glenn Res Ctr, Cleveland, OH 44135 USA. EM alp.sehirlioglu@case.edu FU Air Force Office of Scientific Research [FA 9550-06-1-0260] FX This work was supported by the Air Force Office of Scientific Research under Grant No. FA 9550-06-1-0260. NR 10 TC 35 Z9 36 U1 0 U2 27 PU AMER INST PHYSICS PI MELVILLE PA 1305 WALT WHITMAN RD, STE 300, MELVILLE, NY 11747-4501 USA SN 0021-8979 EI 1089-7550 J9 J APPL PHYS JI J. Appl. Phys. PD JUL 1 PY 2009 VL 106 IS 1 AR 014102 DI 10.1063/1.3158542 PG 7 WC Physics, Applied SC Physics GA 471NK UT WOS:000268065000092 ER PT J AU Caiozzo, VJ Haddad, F Lee, S Baker, M Paloski, W Baldwin, KM AF Caiozzo, V. J. Haddad, F. Lee, S. Baker, M. Paloski, William Baldwin, K. M. TI Artificial gravity as a countermeasure to microgravity: a pilot study examining the effects on knee extensor and plantar flexor muscle groups SO JOURNAL OF APPLIED PHYSIOLOGY LA English DT Article DE gene expression; muscle biopsy; messenger ribonucleic acid; anabolic/catabolic markers ID RESISTANCE EXERCISE; SKELETAL-MUSCLE; BED REST; ORTHOSTATIC INTOLERANCE; SPACEFLIGHT; RESPONSES; EXPRESSION; ATROPHY; SPACE; SIZE AB Caiozzo VJ, Haddad F, Lee S, Baker M, Paloski W, Baldwin KM. Artificial gravity as a countermeasure to microgravity: a pilot study examining the effects on knee extensor and plantar flexor muscle groups. J Appl Physiol 107: 39-46, 2009. First published March 12, 2009; doi: 10.1152/japplphysiol.91130.2008.-The goal of this project was to examine the effects of artificial gravity (AG) on skeletal muscle strength and key anabolic/catabolic markers known to regulate muscle mass. Two groups of subjects were selected for study: 1) a 21 day-bed rest (BR) group (n = 7) and 2) an AG group (n = 8), which was subjected to 21 days of 6 degrees head-down tilt bed rest plus daily 1-h exposures to AG (2.5 G at the feet). Centrifugation was produced using a short-arm centrifuge with the foot plate similar to 220 cm from the center of rotation. The torque-velocity relationships of the knee extensors and plantar flexors of the ankle were determined pre- and posttreatment. Muscle biopsy samples obtained from the vastus lateralis and soleus muscles were used for a series of gene expression analyses (mRNA abundance) of key factors implicated in the anabolic vs. catabolic state of the muscle. Post/pre torque-velocity determinations revealed greater decrements in knee extensor performance in the BR vs. AG group (P < 0.04). The plantar flexors of the AG subjects actually demonstrated a net gain in the torque-velocity relationship, whereas in the BR group, the responses declined (AG vs. BR, P < 0.001). Muscle fiber cross-sectional area decreased by similar to 20% in the BR group, whereas no losses were evident in the AG group. RT-PCR analyses of muscle biopsy specimens demonstrated that markers of growth and cytoskeletal integrity were higher in the AG group, whereas catabolic markers were elevated in the BR group. Importantly, these patterns were seen in both muscles. We conclude that paradigms of AG have the potential to maintain the functional, biochemical, and structural homeostasis of skeletal muscle in the face of chronic unloading. C1 [Caiozzo, V. J.; Baker, M.] Univ Calif Irvine, Coll Hlth Sci, Dept Orthopaed, Irvine, CA 92697 USA. [Caiozzo, V. J.; Haddad, F.; Baldwin, K. M.] Univ Calif Irvine, Coll Hlth Sci, Dept Physiol & Biophys, Irvine, CA 92697 USA. [Paloski, William] Univ Houston, Dept Hlth & Human Performance, Houston, TX USA. [Lee, S.] NASA, Lyndon B Johnson Space Ctr, Wyle Labs, Human Performance Lab, Houston, TX 77058 USA. RP Caiozzo, VJ (reprint author), Univ Calif Irvine, Coll Hlth Sci, Dept Orthopaed, Irvine, CA 92697 USA. EM vjcaiozz@uci.edu FU National Aeronautics and Space Administration Human Research Program [NASA-NNJ-068HC6IG]; National Institutes of Health [M01 RR0073] FX This study was supported by National Aeronautics and Space Administration Human Research Program Grant NASA-NNJ-068HC6IG (to K. M. Baldwin) and was conducted at the National Institutes of Health-funded (M01 RR0073) GCRC at UTMB, Galveston, TX. NR 40 TC 29 Z9 30 U1 0 U2 6 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 JUL PY 2009 VL 107 IS 1 BP 39 EP 46 DI 10.1152/japplphysiol.91130.2008 PG 8 WC Physiology; Sport Sciences SC Physiology; Sport Sciences GA 464VK UT WOS:000267535800008 PM 19286573 ER PT J AU Smith, SM Zwart, SR Heer, MA Baecker, N Evans, HJ Feiveson, AH Shackelford, LC LeBlanc, AD AF Smith, S. M. Zwart, S. R. Heer, M. A. Baecker, N. Evans, H. J. Feiveson, A. H. Shackelford, L. C. LeBlanc, A. D. TI Effects of artificial gravity during bed rest on bone metabolism in humans SO JOURNAL OF APPLIED PHYSIOLOGY LA English DT Article DE microgravity; countermeasure; bone resorption; bone formation ID BODY NEGATIVE-PRESSURE; SPACE-FLIGHT; SIMULATED MICROGRAVITY; TREADMILL EXERCISE; CALCIUM EXCRETION; NUTRITIONAL-STATUS; MECHANICAL STRAIN; IDENTICAL-TWINS; MINERAL DENSITY; RESORPTION AB Smith SM, Zwart SR, Heer MA, Baecker N, Evans HJ, Feiveson AH, Shackelford LC, LeBlanc AD. Effects of artificial gravity during bed rest on bone metabolism in humans. J Appl Physiol 107: 47-53, 2009. First published December 12, 2008; doi: 10.1152/japplphysiol.91134.2008.-We report results from a study designed to explore the utility of artificial gravity (AG) as a countermeasure to bone loss induced by microgravity simulation. After baseline testing, 15 male subjects underwent 21 days of 6 head-down bed rest to simulate the deconditioning associated with spaceflight. Eight of the subjects underwent 1 h of centrifugation (AG; 1 G(z) at the heart, 2.5 G(z) at the feet) each day for 21 days, whereas seven of the subjects served as untreated controls (Con). Blood and urine were collected before, during, and after bed rest for bone marker determinations. Bone mineral density (BMD) and bone mineral content (BMC) were determined by dual-energy X-ray absorptiometry and peripheral quantitative computerized tomography before and after bed rest. Urinary excretion of bone resorption markers increased during bed rest, but the AG and Con groups did not differ significantly. The same was true for serum C-telopeptide. During bed rest, bone alkaline phosphatase (ALP) and total ALP tended to be lower in the AG group (P = 0.08, P = 0.09). Neither BMC nor BMD changed significantly from the pre-bed rest period in AG or Con groups, and the two groups were not significantly different. However, when AG and Con data were combined, there was a significant (P < 0.05) effect of time for whole body total BMC and total hip and trochanter BMD. These data failed to demonstrate efficacy of this AG prescription to prevent the changes in bone metabolism observed during 3 wk of bed rest. C1 [Smith, S. M.; Feiveson, A. H.; Shackelford, L. C.] NASA, Lyndon B Johnson Space Ctr, Human Adaptat & Countermeasures Div, Houston, TX 77058 USA. [Zwart, S. R.; LeBlanc, A. D.] Univ Space Res Assoc, Houston, TX USA. [Heer, M. A.; Baecker, N.] German Aerosp Ctr, Inst Aerosp Med, Cologne, Germany. RP Smith, SM (reprint author), NASA, Lyndon B Johnson Space Ctr, Human Adaptat & Countermeasures Div, Attn Mail Code SK3,2101 NASA Pkwy, Houston, TX 77058 USA. EM scott.m.smith@nasa.gov FU NASA Human Research Program; National Institutes of Health-funded [M01 RR 0073] FX This work was funded by the NASA Human Research Program and was conducted at the National Institutes of Health-funded (M01 RR 0073) General Clinical Research Center at the University of Texas Medical Branch, Galveston, TX. NR 57 TC 31 Z9 32 U1 0 U2 8 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 JUL PY 2009 VL 107 IS 1 BP 47 EP 53 DI 10.1152/japplphysiol.91134.2008 PG 7 WC Physiology; Sport Sciences SC Physiology; Sport Sciences GA 464VK UT WOS:000267535800009 PM 19074572 ER PT J AU Zwart, SR Crawford, GE Gillman, PL Kala, G Rodgers, AS Rogers, A Inniss, AM Rice, BL Ericson, K Coburn, S Bourbeau, Y Hudson, E Mathew, G DeKerlegand, DE Sams, CF Heer, MA Paloski, WH Smith, SM AF Zwart, S. R. Crawford, G. E. Gillman, P. L. Kala, G. Rodgers, A. S. Rogers, A. Inniss, A. M. Rice, B. L. Ericson, K. Coburn, S. Bourbeau, Y. Hudson, E. Mathew, G. DeKerlegand, D. E. Sams, C. F. Heer, M. A. Paloski, W. H. Smith, S. M. TI Effects of 21 days of bed rest, with or without artificial gravity, on nutritional status of humans SO JOURNAL OF APPLIED PHYSIOLOGY LA English DT Article DE microgravity; countermeasure; vitamin E; beta-carotene; vitamin B(6) ID RED-BLOOD-CELLS; SPACE-FLIGHT; SIMULATED WEIGHTLESSNESS; ENERGY-EXPENDITURE; HIGH-SALT; SPACEFLIGHT; METABOLISM; RISK; ACID; HYPERGRAVITY AB Zwart SR, Crawford GE, Gillman PL, Kala G, Rodgers AS, Rogers A, Inniss AM, Rice BL, Ericson K, Coburn S, Bourbeau Y, Hudson E, Mathew G, DeKerlegand DE, Sams CF, Heer MA, Paloski WH, Smith SM. Effects of 21 days of bed rest, with or without artificial gravity, on nutritional status of humans. J Appl Physiol 107: 54-62, 2009. First published December 12, 2008; doi: 10.1152/japplphysiol.91136.2008.-Spaceflight and bed rest models of microgravity have profound effects on physiological systems, including the cardiovascular, musculoskeletal, and immune systems. These effects can be exacerbated by suboptimal nutrient status, and therefore it is critical to monitor nutritional status when evaluating countermeasures to mitigate negative effects of spaceflight. As part of a larger study to investigate the usefulness of artificial gravity as a countermeasure for musculoskeletal and cardiovascular deficits during bed rest, we tested the hypothesis that artificial gravity would have an effect on some aspects of nutritional status. Dietary intake was recorded daily before, during, and after 21 days of bed rest with artificial gravity (n = 8) or bed rest alone (n = 7). We examined body composition, hematology, general blood chemistry, markers of oxidative damage, and blood levels of selected vitamins and minerals before, during, and after the bed rest period. Several indicators of vitamin status changed in response to diet changes: serum alpha- and gamma-tocopherol and urinary 4-pyridoxic acid decreased (P < 0.001) and plasma beta-carotene increased (P < 0.001) in both groups during bed rest compared with before bed rest. A decrease in hematocrit (P < 0.001) after bed rest was accompanied by a decrease in transferrin (P < 0.001), but transferrin receptors were not changed. These data provide evidence that artificial gravity itself does not negatively affect nutritional status during bed rest. Likewise, artificial gravity has no protective effect on nutritional status during bed rest. C1 [Sams, C. F.; Paloski, W. H.; Smith, S. M.] NASA, Lyndon B Johnson Space Ctr, Human Adaptat & Countermeasures Div, Houston, TX 77058 USA. [Heer, M. A.] German Aerosp Ctr, Inst Aerosp Med, Cologne, Germany. [Hudson, E.] JES Tech, Houston, TX USA. [Ericson, K.; Coburn, S.] Indiana Univ Purdue Univ, Dept Chem, Ft Wayne, IN 46805 USA. [Inniss, A. M.] Univ Texas Med Branch, Galveston, TX USA. [Crawford, G. E.; Gillman, P. L.; Kala, G.; Rodgers, A. S.; Rogers, A.; Rice, B. L.; Bourbeau, Y.; Mathew, G.; DeKerlegand, D. E.] Enterprise Advisory Serv Inc, Houston, TX USA. [Zwart, S. R.] Univ Space Res Assoc, Houston, TX USA. RP Smith, SM (reprint author), NASA, Lyndon B Johnson Space Ctr, Human Adaptat & Countermeasures Div, Attn Mail Code SK3,2101 NASA Pkwy, Houston, TX 77058 USA. EM scott.m.smith@nasa.gov FU NASA; U. S. Department of Agriculture agreement [58-1950-4-401] FX This work was funded by NASA and by U. S. Department of Agriculture agreement no. 58-1950-4-401. Any opinions, findings, conclusions, or recommendations expressed in this publication are those of the authors and do not necessarily reflect the view of the U. S. Department of Agriculture. NR 53 TC 25 Z9 25 U1 0 U2 6 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 JUL PY 2009 VL 107 IS 1 BP 54 EP 62 DI 10.1152/japplphysiol.91136.2008 PG 9 WC Physiology; Sport Sciences SC Physiology; Sport Sciences GA 464VK UT WOS:000267535800010 PM 19074571 ER PT J AU Liu, ZY Vaughan, M Winker, D Kittaka, C Getzewich, B Kuehn, R Omar, A Powell, K Trepte, C Hostetler, C AF Liu, Zhaoyan Vaughan, Mark Winker, David Kittaka, Chieko Getzewich, Brian Kuehn, Ralph Omar, Ali Powell, Kathleen Trepte, Charles Hostetler, Chris TI The CALIPSO Lidar Cloud and Aerosol Discrimination: Version 2 Algorithm and Initial Assessment of Performance SO JOURNAL OF ATMOSPHERIC AND OCEANIC TECHNOLOGY LA English DT Article ID BACKSCATTER; EXTINCTION; DUST; RETRIEVAL; LITE AB The Cloud-Aerosol Lidar and Infrared Pathfinder Satellite Observations (CALIPSO) satellite was launched in April 2006 to provide global vertically resolved measurements of clouds and aerosols. Correct discrimination between clouds and aerosols observed by the lidar aboard the CALIPSO satellite is critical for accurate retrievals of cloud and aerosol optical properties and the correct interpretation of measurements. This paper reviews the theoretical basis of the CALIPSO lidar cloud and aerosol discrimination (CAD) algorithm, and describes the enhancements made to the version 2 algorithm that is used in the current data release (release 2). The paper also presents a preliminary assessment of the CAD performance based on one full day (12 August 2006) of expert manual classification and on one full month (July 2006) of the CALIOP 5-km cloud and aerosol layer products. Overall, the CAD algorithm works well in most cases. The 1-day manual verification suggests that the success rate is in the neighborhood of 90% or better. Nevertheless, several specific layer types are still misclassified with some frequency. Among these, the most prevalent are dense dust and smoke close to the source regions. The analysis of the July 2006 data showed that the misclassification of dust as cloud occurs for < 1% of the total tropospheric cloud and aerosol features found. Smoke layers are misclassified less frequently than are dust layers. Optically thin clouds in the polar regions can be misclassified as aerosols. While the fraction of such misclassifications is small compared with the number of aerosol features found globally, caution should be taken when studies are performed on the aerosol in the polar regions. Modifications will be made to the CAD algorithm in future data releases, and the misclassifications encountered in the current data release are expected to be reduced greatly. C1 [Liu, Zhaoyan] Natl Inst Aerosp, Hampton, VA USA. [Vaughan, Mark; Winker, David; Omar, Ali; Powell, Kathleen; Trepte, Charles; Hostetler, Chris] NASA, Hampton, VA USA. [Kittaka, Chieko; Getzewich, Brian; Kuehn, Ralph] Sci Syst & Applicat Inc, Hampton, VA USA. RP Liu, ZY (reprint author), 100 Explorat Way, Hampton, VA 23666 USA. EM zhaoyan.liu-1@nasa.gov RI Liu, Zhaoyan/B-1783-2010; Liu, Zhaoyan/A-9604-2009; Omar, Ali/D-7102-2017 OI Liu, Zhaoyan/0000-0003-4996-5738; Omar, Ali/0000-0003-1871-9235 NR 37 TC 176 Z9 180 U1 6 U2 36 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 JUL PY 2009 VL 26 IS 7 BP 1198 EP 1213 DI 10.1175/2009JTECHA1229.1 PG 16 WC Engineering, Ocean; Meteorology & Atmospheric Sciences SC Engineering; Meteorology & Atmospheric Sciences GA 479LX UT WOS:000268662000003 ER PT J AU Hunt, WH Winker, DM Vaughan, MA Powell, KA Lucker, PL Weimer, C AF Hunt, William H. Winker, David M. Vaughan, Mark A. Powell, Kathleen A. Lucker, Patricia L. Weimer, Carl TI CALIPSO Lidar Description and Performance Assessment SO JOURNAL OF ATMOSPHERIC AND OCEANIC TECHNOLOGY LA English DT Article ID MISSION; CLOUDS AB This paper provides background material for a collection of Cloud-Aerosol Lidar with Orthogonal Polarization (CALIOP) algorithm papers that are to be published in the Journal of Atmospheric and Oceanic Technology. It provides a brief description of the design and performance of CALIOP, a three-channel elastic backscatter lidar on the Cloud-Aerosol Lidar and Infrared Pathfinder Satellite Observation (CALIPSO) satellite. After more than 2 yr of on-orbit operation, CALIOP performance continues to be excellent in the key areas of laser energy, signal-to-noise ratio, polarization sensitivity, and overall long-term stability, and the instrument continues to produce high-quality data products. There are, however, some areas where performance has been less than ideal. These include short-term changes in the calibration coefficients at both wavelengths as the satellite passes between dark and sunlight, some radiation-induced effects on both the detectors and the laser when passing through the South Atlantic Anomaly, and slow transient recovery on the 532-nm channels. Although these issues require some special treatment in data analysis, they do not seriously detract from the overall quality of the level 2 data products. C1 [Hunt, William H.; Lucker, Patricia L.] Sci Syst & Applicat Inc, Hampton, VA USA. [Winker, David M.; Vaughan, Mark A.; Powell, Kathleen A.] NASA, Hampton, VA USA. [Weimer, Carl] Ball Aerosp & Technology Corp, Boulder, CO USA. RP Hunt, WH (reprint author), NASA, Langley Res Ctr, MS 475, Hampton, VA 23681 USA. EM william.h.hunt@nasa.gov NR 17 TC 158 Z9 161 U1 4 U2 33 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 JUL PY 2009 VL 26 IS 7 BP 1214 EP 1228 DI 10.1175/2009JTECHA1223.1 PG 15 WC Engineering, Ocean; Meteorology & Atmospheric Sciences SC Engineering; Meteorology & Atmospheric Sciences GA 479LX UT WOS:000268662000004 ER PT J AU Matsui, T Zeng, XP Tao, WK Masunaga, H Olson, WS Lang, S AF Matsui, Toshihisa Zeng, Xiping Tao, Wei-Kuo Masunaga, Hirohiko Olson, William S. Lang, Stephen TI Evaluation of Long-Term Cloud-Resolving Model Simulations Using Satellite Radiance Observations and Multifrequency Satellite Simulators SO JOURNAL OF ATMOSPHERIC AND OCEANIC TECHNOLOGY LA English DT Article ID TROPICAL CONVECTION; OCEANIC CONVECTION; RADIATIVE-TRANSFER; PART I; PRECIPITATION; SENSITIVITY; ALGORITHM; SYSTEMS; RADAR; UNCERTAINTIES AB This paper proposes a methodology known as the Tropical Rainfall Measuring Mission (TRMM) Triple-Sensor Three-Step Evaluation Framework (T3EF) for the systematic evaluation of precipitating cloud types and microphysics in a cloud-resolving model (CRM). T3EF utilizes multisensor satellite simulators and novel statistics of multisensor radiance and backscattering signals observed from the TRMM satellite. Specifically, T3EF compares CRM and satellite observations in the form of combined probability distributions of precipitation radar (PR) reflectivity, polarization-corrected microwave brightness temperature (T(b)), and infrared T(b) to evaluate the candidate CRM. T3EF is used to evaluate the Goddard Cumulus Ensemble (GCE) model for cases involving the South China Sea Monsoon Experiment (SCSMEX) and the Kwajalein Experiment (KWAJEX). This evaluation reveals that the GCE properly captures the satellite-measured frequencies of different precipitating cloud types in the SCSMEX case but overestimates the frequencies of cumulus congestus in the KWAJEX case. Moreover, the GCE tends to simulate excessively large and abundant frozen condensates in deep precipitating clouds as inferred from the overestimated GCE-simulated radar reflectivities and microwave T(b) depressions. Unveiling the detailed errors in the GCE's performance provides the better direction for model improvements. C1 [Matsui, Toshihisa; Zeng, Xiping; Tao, Wei-Kuo; Olson, William S.; Lang, Stephen] NASA, Goddard Space Flight Ctr, Atmospheres Lab, Greenbelt, MD 20771 USA. [Matsui, Toshihisa; Zeng, Xiping] Univ Maryland Baltimore Cty, Goddard Earth Sci & Technol Ctr, Baltimore, MD 21228 USA. [Masunaga, Hirohiko] Nagoya Univ, Hydrospher Atmospher Res Ctr, Nagoya, Aichi 4648601, Japan. [Olson, William S.] Univ Maryland Baltimore Cty, Joint Ctr Earth Syst Technol, Baltimore, MD 21228 USA. [Lang, Stephen] Sci Syst & Applicat Inc, Lanham, MD USA. RP Matsui, T (reprint author), NASA, Goddard Space Flight Ctr, Atmospheres Lab, Code 613-1, Greenbelt, MD 20771 USA. EM toshihisa_matsui-1@nasa.gov RI Masunaga, Hirohiko/C-2488-2008; PMM, JAXA/K-8537-2016 OI Masunaga, Hirohiko/0000-0002-6336-5002; FU NASA Headquarters Atmospheric Dynamics and Thermodynamics Program; NASA Tropical Rainfall Measuring Mission (TRMM) FX This research was supported by the NASA Headquarters Atmospheric Dynamics and Thermodynamics Program and the NASA Tropical Rainfall Measuring Mission (TRMM). The authors are grateful to Dr. R. Kakar at NASA HQ for his support of this research. This program was also supported by the NASA MAP program. The authors are grateful to Dr. D. Anderson at NASA HQ. The authors also acknowledge NASA GSFC and Ames Research Center for computer time used in this research, and thank Wesley Berg and two anonymous reviewers and an editor for their constructive comments and suggestions. NR 31 TC 41 Z9 41 U1 0 U2 6 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 JUL PY 2009 VL 26 IS 7 BP 1261 EP 1274 DI 10.1175/2008JTECHA1168.1 PG 14 WC Engineering, Ocean; Meteorology & Atmospheric Sciences SC Engineering; Meteorology & Atmospheric Sciences GA 479LX UT WOS:000268662000007 ER PT J AU Chao, Y Li, ZJ Farrara, JD Hung, P AF Chao, Yi Li, Zhijin Farrara, John D. Hung, Peter TI Blending Sea Surface Temperatures from Multiple Satellites and In Situ Observations for Coastal Oceans SO JOURNAL OF ATMOSPHERIC AND OCEANIC TECHNOLOGY LA English DT Article ID SYSTEM; INTERPOLATION; ACCURACY; CLIMATE; SST AB A two-dimensional variational data assimilation (2DVAR) method for blending sea surface temperature (SST) data from multiple observing platforms is presented. This method produces continuous fields and has the capability of blending multiple satellite and in situ observations. In addition, it allows specification of inhomogeneous and anisotropic background correlations, which are common features of coastal ocean flows. High-resolution ( 6 km in space and 6 h in time) blended SST fields for August 2003 are produced for a region off the California coast to demonstrate and evaluate the methodology. A comparison of these fields with independent observations showed root-mean-square errors of less than 1 degrees C, comparable to the errors in conventional SST observations. The blended SST fields also clearly reveal the finescale spatial and temporal structures associated with coastal upwelling, demonstrating their utility in the analysis of finescale flows. With the high temporal resolution, the blended SST fields are also used to describe the diurnal cycle. Potential applications of this SST blending methodology in other coastal regions are discussed. C1 [Chao, Yi; Li, Zhijin] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Farrara, John D.] Univ Calif Los Angeles, Joint Inst Reg Earth Syst Sci & Engn, Los Angeles, CA USA. RP Chao, Y (reprint author), CALTECH, Jet Prop Lab, M-S 183-601,4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM yi.chao@jpl.nasa.gov FU Office of Naval Research (ONR) FX The research described in this publication was carried out, in part, by the Jet Propulsion Laboratory (JPL), California Institute of Technology, under a contract with the National Aeronautics and Space Administration ( NASA). The AMSR-E and TMI SSTs were provided by Remote Sensing Systems ( available online at http://www.ssmi.com). The GOES and MC SSTs were provided by PO. DAAC ( available online at http://podaac.jpl.nasa.gov). The in situ observations were provided by the Global Ocean Data Assimilation Experiment (GODAE; available online at http://www.usgodae.org). Support from the Office of Naval Research (ONR) through a subcontract from the Monterey Bay Aquarium Research Institute (MBARI) is acknowledged. We thank Drs. J. Vazquez and E. Armstrong for useful discussion. The comments of two anonymous reviewers contributed to improve the original manuscript. NR 22 TC 22 Z9 23 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 JUL PY 2009 VL 26 IS 7 BP 1415 EP 1426 DI 10.1175/2009JTECHO592.1 PG 12 WC Engineering, Ocean; Meteorology & Atmospheric Sciences SC Engineering; Meteorology & Atmospheric Sciences GA 479LX UT WOS:000268662000021 ER PT J AU Denton, MH Borovsky, JE Horne, RB McPherron, RL Morley, SK Tsurutani, BT AF Denton, M. H. Borovsky, J. E. Horne, R. B. McPherron, R. L. Morley, S. K. Tsurutani, B. T. TI Introduction to Special Issue on high speed solar wind streams and geospace interactions (HSS-GI) SO JOURNAL OF ATMOSPHERIC AND SOLAR-TERRESTRIAL PHYSICS LA English DT Editorial Material C1 [Denton, M. H.] Univ Lancaster, Dept Commun Syst, Lancaster, England. [Borovsky, J. E.] Los Alamos Natl Lab, Los Alamos, NM USA. [Horne, R. B.] British Antarctic Survey, Cambridge CB3 0ET, England. [McPherron, R. L.] Univ Calif Los Angeles, IGPP, Los Angeles, CA USA. [Morley, S. K.] Univ Newcastle, Newcastle, NSW 2308, Australia. [Tsurutani, B. T.] CALTECH, Jet Prop Lab, Pasadena, CA USA. RP Denton, MH (reprint author), Univ Lancaster, Dept Commun Syst, Lancaster, England. EM m.denton@lancaster.ac.uk RI Morley, Steven/A-8321-2008; OI Morley, Steven/0000-0001-8520-0199; Horne, Richard/0000-0002-0412-6407; Denton, Michael/0000-0002-1748-3710 NR 19 TC 7 Z9 7 U1 2 U2 3 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 JUL PY 2009 VL 71 IS 10-11 SI SI BP 1011 EP 1013 DI 10.1016/j.jastp.2008.09.019 PG 3 WC Geochemistry & Geophysics; Meteorology & Atmospheric Sciences SC Geochemistry & Geophysics; Meteorology & Atmospheric Sciences GA 478QE UT WOS:000268602100001 ER PT J AU Emery, BA Richardson, IG Evans, DS Rich, FJ AF Emery, Barbara A. Richardson, Ian G. Evans, David S. Rich, Frederick J. TI Solar wind structure sources and periodicities of auroral electron power over three solar cycles SO JOURNAL OF ATMOSPHERIC AND SOLAR-TERRESTRIAL PHYSICS LA English DT Article; Proceedings Paper CT Workshop on High Speed Solar Wind Streams and Geospace Interactions CY SEP 02-07, 2007 CL St Martins Coll, Ambleside, ENGLAND HO St Martins Coll DE Electron auroral energy fluxes; Solar wind speed structures; Solar cycle variations; Periodicities ID INTERPLANETARY MAGNETIC-FIELD; CORONAL MASS EJECTIONS; PREFERRED BARTELS DAYS; SPEED PLASMA STREAMS; FLUX-TRANSFER EVENTS; GEOMAGNETIC-ACTIVITY; SPECTRAL-ANALYSIS; SEMIANNUAL VARIATION; STATISTICAL-MODEL; SPACED DATA AB We assess the contributions of various types of solar wind structures (transients, coronal hole high-speed streams (HSS), and slow-speed wind) to hourly average auroral electron power (P(e)) The time variation of the solar wind velocity (V(sw)) and P(e) are determined by HSS, which contribute similar to 47% to P(e) and V(sw). Transients contribute similar to 42% of P(e) in solar maxima, and similar to 6% in solar minimum. Cross-correlations of P(e) with V(sw)vertical bar B vertical bar for negative B(z) are significant. P. exhibits solar rotational periodicities similar to those for V(sw) with strong 7- and 9-day periodicities in 2005-2008 and equinox semiannual periodicities in 1995-1999. (C) 2008 Elsevier Ltd. All rights reserved. C1 [Emery, Barbara A.] Natl Ctr Atmospher Res, High Altitude Observ, Boulder, CO 80307 USA. [Richardson, Ian G.] NASA, Goddard Space Flight Ctr, Bethesda, MD USA. [Richardson, Ian G.] Univ Maryland, College Pk, MD 20742 USA. [Evans, David S.] NOAA, Space Weather Predict Ctr, Boulder, CO USA. RP Emery, BA (reprint author), Natl Ctr Atmospher Res, High Altitude Observ, Pob 3000, Boulder, CO 80307 USA. EM emery@hao.ucar.edu OI Richardson, Ian/0000-0002-3855-3634 NR 87 TC 48 Z9 48 U1 0 U2 4 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 JUL PY 2009 VL 71 IS 10-11 BP 1157 EP 1175 DI 10.1016/j.jastp.2008.08.005 PG 19 WC Geochemistry & Geophysics; Meteorology & Atmospheric Sciences SC Geochemistry & Geophysics; Meteorology & Atmospheric Sciences GA 478QE UT WOS:000268602100013 ER PT J AU Lebassi, B Gonzalez, J Fabris, D Maurer, E Miller, N Milesi, C Switzer, P Bornstein, R AF Lebassi, Bereket Gonzalez, Jorge Fabris, Drazen Maurer, Edwin Miller, Norman Milesi, Cristina Switzer, Paul Bornstein, Robert TI Observed 1970-2005 Cooling of Summer Daytime Temperatures in Coastal California SO JOURNAL OF CLIMATE LA English DT Article ID INDUCED CLIMATE-CHANGE; MONTANE CLOUD FORESTS; SURFACE-TEMPERATURE; LOWLAND DEFORESTATION; MINIMUM TEMPERATURE; GLOBAL CLIMATE; LAND-USE; TRENDS; IMPACTS; METHODOLOGY AB This study evaluated 1950-2005 summer [June-August (JJA)] mean monthly air temperatures for two California air basins: the South Coast Air Basin (SoCAB) and the San Francisco Bay Area (SFBA). The study focuses on the more rapid post-1970 warming period, and its daily minima temperature T-min and maxima temperature T-max values were used to produce average monthly values and spatial distributions of trends for each air basin. Additional analyses included concurrent SSTs, 40-yr European Centre for Medium-Range Weather Forecasts (ECMWF) Re-Analysis (ERA-40) sea level coastal pressure gradients, and GCM-downscaled average temperature T-ave values. Results for all 253 California National Weather Service (NWS) Cooperative Observer Program (COOP) sites together showed increased T-ave values (0.238 degrees C decade(-1)); asymmetric warming, as T-min values increase faster than T-max values (0.27 degrees versus 0.04 degrees C decade(-1)) and thus decreased daily temperature range (DTR) values (0.15 degrees C decade(-1)). The spatial distribution of observed SoCAB and SFBA T-max values exhibited a complex pattern, with cooling (-0.30 degrees C decade(-1)) in low-elevation coastal areas open to marine air penetration and warming (0.32 degrees C decade(-1)) in inland areas. Results also showed that decreased DTR values in the basins arose from small increases at inland sites (0.16 degrees C decade(-1)) combined with large decreases (20.58 degrees C decade(-1)) at coastal sites. It is also possible that some of the current observed temperature trends could be associated with low-frequency decadal variability, expected even with a constant radiative forcing. Previous studies suggest that cooling JJA T-max values in coastal California were a result of increased irrigation, coastal upwelling, or cloud cover. The current hypothesis is that they arise (as a possible "reverse reaction'') from the global warming of inland areas, which results in increased sea-breeze flow activity. GCM model T-ave warming decreased from 0.13 degrees C decade(-1) at inland sites to 0.08 degrees C decade(-1) in coastal areas. Sea level pressure increased in the Pacific high and decreased in the thermal low. The corresponding gradient thus showed a trend of 0.04 hPa 100 km(-1) decade(-1), supportive of the hypothesis of increased sea-breeze activity. C1 [Lebassi, Bereket; Gonzalez, Jorge; Fabris, Drazen] Santa Clara Univ, Dept Mech Engn, Santa Clara, CA 95053 USA. [Maurer, Edwin] Santa Clara Univ, Dept Civil Engn, Santa Clara, CA 95053 USA. [Miller, Norman] Lawrence Berkeley Natl Lab, Climate Sci Dept, Berkeley, CA USA. [Milesi, Cristina] NASA, Ames Res Ctr, Mountain View, CA USA. [Milesi, Cristina] Univ Corp Monterey Bay, Seaside, CA USA. [Switzer, Paul] Stanford Univ, Dept Stat, Stanford, CA 94305 USA. [Switzer, Paul] Stanford Univ, Dept Environm & Earth Syst Sci, Stanford, CA 94305 USA. [Bornstein, Robert] San Jose State Univ, Dept Meteorol, San Jose, CA 95192 USA. RP Gonzalez, J (reprint author), CUNY, NOAA, CREST, Steinman Hall T-238, New York, NY 10031 USA. EM gonzalez@me.ccny.cuny.edu RI Maurer, Edwin/C-7190-2009; Miller, Norman/E-6897-2010 OI Maurer, Edwin/0000-0001-7134-487X; FU Program for Climate Model Diagnosis and Intercomparison (PCMDI); WCRP Working Group on Coupled Modelling (WGCM); Office of Science, U.S. Department of Energy FX The authors thank Prof. Alan Robock of Rutgers University for his insightful comments. We also thank the School of Engineering, Santa Clara University for funding the lead author. We also acknowledge the Program for Climate Model Diagnosis and Intercomparison (PCMDI) for collecting and archiving CMIP3 model output and the WCRP Working Group on Coupled Modelling (WGCM) for organizing the model data analysis. The WCRP CMIP3 multimodel dataset is supported by the Office of Science, U.S. Department of Energy. NR 55 TC 36 Z9 36 U1 4 U2 16 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 JUL PY 2009 VL 22 IS 13 BP 3558 EP 3573 DI 10.1175/2008JCLI2111.1 PG 16 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 472JQ UT WOS:000268127300003 ER PT J AU Ravi, V Firdosy, S Caillat, T Brandon, E Van der Walde, K Maricic, L Sayir, A AF Ravi, Vilupanur Firdosy, Samad Caillat, Thierry Brandon, Erik Van der Walde, Keith Maricic, Lina Sayir, Ali TI Thermal Expansion Studies of Selected High-Temperature Thermoelectric Materials SO JOURNAL OF ELECTRONIC MATERIALS LA English DT Article; Proceedings Paper CT 27th International Conference on Thermoelectrics CY AUG 03-07, 2008 CL Univ Oregon, Corvallis, OR SP Int Thermoelect Soc HO Univ Oregon DE Thermoelectrics; thermal expansion; silicon germanium; Yb(14)MnSb(11); skutterudites; thermomechanical modeling ID RESIDUAL-STRESSES; COATINGS AB Radioisotope thermoelectric generators (RTGs) generate electrical power by converting the heat released from the nuclear decay of radioactive isotopes (typically plutonium-238) into electricity using a thermoelectric converter. RTGs have been successfully used to power a number of space missions and have demonstrated their reliability over an extended period of time (tens of years) and are compact, rugged, radiation resistant, scalable, and produce no noise, vibration or torque during operation. System conversion efficiency for state-of-practice RTGs is about 6% and specific power a parts per thousand currency sign5.1 W/kg. A higher specific power would result in more onboard power for the same RTG mass, or less RTG mass for the same onboard power. The Jet Propulsion Laboratory has been leading, under the advanced thermoelectric converter (ATEC) project, the development of new high-temperature thermoelectric materials and components for integration into advanced, more efficient RTGs. Thermoelectric materials investigated to date include skutterudites, the Yb(14)MnSb(11) compound, and SiGe alloys. The development of long-lived thermoelectric couples based on some of these materials has been initiated and is assisted by a thermomechanical stress analysis to ensure that all stresses under both fabrication and operation conditions will be within yield limits for those materials. Several physical parameters are needed as input to this analysis. Among those parameters, the coefficient of thermal expansion (CTE) is critically important. Thermal expansion coefficient measurements of several thermoelectric materials under consideration for ATEC are described in this paper. The stress response at the interfaces in material stacks subjected to changes in temperature is discussed, drawing on work from the literature and project-specific tools developed here. The degree of CTE mismatch and the associated effect on the formation of stress is highlighted. C1 [Ravi, Vilupanur; Firdosy, Samad; Caillat, Thierry; Brandon, Erik] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Ravi, Vilupanur] Calif State Polytech Univ Pomona, Pomona, CA 91768 USA. [Van der Walde, Keith; Maricic, Lina] ATA Engn Inc, San Diego, CA 92130 USA. [Sayir, Ali] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. RP Ravi, V (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM varavi@jpl.nasa.gov NR 14 TC 35 Z9 36 U1 4 U2 34 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0361-5235 J9 J ELECTRON MATER JI J. Electron. Mater. PD JUL PY 2009 VL 38 IS 7 BP 1433 EP 1442 DI 10.1007/s11664-009-0734-2 PG 10 WC Engineering, Electrical & Electronic; Materials Science, Multidisciplinary; Physics, Applied SC Engineering; Materials Science; Physics GA 466LA UT WOS:000267662500097 ER PT J AU Hogue, MD Calle, CI Curry, DR Weitzman, PS AF Hogue, M. D. Calle, C. I. Curry, D. R. Weitzman, P. S. TI Discrete element modeling (DEM) of triboelectrically charged particles: Revised experiments SO JOURNAL OF ELECTROSTATICS LA English DT Article DE Triboelectric; Particles; Discrete element modeling; Charge generation coefficient AB In a previous work, the addition of basic screened Coulombic electrostatic forces to an existing commercial discrete element modeling (DEM) software was reported. Triboelectric experiments were performed to charge glass spheres rolling on inclined planes of various materials. Charge generation constants and the Q/m ratios for the test materials were calculated from the experimental data and compared to the simulation output of the DEM software. In this paper, we will discuss new values of the charge generation constants calculated from improved experimental procedures and data. Published by Elsevier B.V. C1 [Hogue, M. D.; Calle, C. I.] NASA, Electrostat & Surface Phys Lab, Kennedy Space Ctr, FL 32899 USA. [Curry, D. R.] DEM Solut Inc, Edinburgh EH1 3EP, Midlothian, Scotland. [Weitzman, P. S.] DEM Solut USA Inc, Lebanon, NH 03766 USA. RP Hogue, MD (reprint author), NASA, Electrostat & Surface Phys Lab, KT B-1, Kennedy Space Ctr, FL 32899 USA. EM michael.d.hogue@nasa.gov; carlos.i.calle@nasa.gov; dcurry@dem-solutions.com NR 8 TC 11 Z9 12 U1 1 U2 6 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0304-3886 J9 J ELECTROSTAT JI J. Electrost. PD JUL PY 2009 VL 67 IS 4 BP 691 EP 694 DI 10.1016/j.elstat.2009.03.005 PG 4 WC Engineering, Electrical & Electronic SC Engineering GA 462YL UT WOS:000267394900022 ER PT J AU Gross, RS AF Gross, Richard S. TI An improved empirical model for the effect of long-period ocean tides on polar motion SO JOURNAL OF GEODESY LA English DT Article DE Earth rotation; Polar motion; Ocean tides; Oceanic angular momentum; Atmospheric angular Momentum ID TIDAL ANGULAR-MOMENTUM; EARTHS ROTATION; EXCITATION; VOLUME AB Because the tide-raising potential is symmetric about the Earth's polar axis it can excite polar motion only by acting upon non-axisymmetric features of the Earth like the oceans. In fact, after removing atmospheric and non-tidal oceanic effects, polar motion excitation observations show a strong fortnightly tidal signal that is not completely explained by existing dynamical and empirical ocean tide models. So a new empirical model for the effect of the termensual (Mtm and mtm), fortnightly (Mf and mf), and monthly (Mm) tides on polar motion is derived here by fitting periodic terms at these tidal frequencies to polar motion excitation observations that span 2 January 1980 to 8 September 2006 and from which atmospheric and non-tidal oceanic effects have been removed. While this new empirical tide model can fully explain the observed fortnightly polar motion excitation signal during this time interval it would still be desirable to have a model for the effect of long-period ocean tides on polar motion that is determined from a dynamical ocean tide model and that is therefore independent of polar motion observations. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Gross, RS (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM Richard.Gross@jpl.nasa.gov FU Jet Propulsion Laboratory; California Institute of Technology; National Aeronautics and Space Administration; NASA's Science Mission Directorate FX I thank S. Dickman for his thoughtful review that led to many improvements to this manuscript. The work described in this paper was performed at the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. Support for this work was provided by the Earth Surface and Interior Focus Area of NASA's Science Mission Directorate. The supercomputers used in this investigation were provided by funding from the JPL Office of the Chief Information Officer. NR 25 TC 17 Z9 18 U1 1 U2 2 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0949-7714 J9 J GEODESY JI J. Geodesy PD JUL PY 2009 VL 83 IS 7 BP 635 EP 644 DI 10.1007/s00190-008-0277-y PG 10 WC Geochemistry & Geophysics; Remote Sensing SC Geochemistry & Geophysics; Remote Sensing GA 460WP UT WOS:000267222700003 ER PT J AU Dow, JM Neilan, RE Rizos, C AF Dow, John M. Neilan, R. E. Rizos, C. TI The International GNSS Service in a changing landscape of Global Navigation Satellite Systems (vol 83, pg 191, 2009) SO JOURNAL OF GEODESY LA English DT Correction C1 [Dow, John M.] ESA ESOC, Darmstadt, Germany. [Neilan, R. E.] NASA JPL, Pasadena, CA USA. [Rizos, C.] Univ New S Wales, Sch Surveying & Spatial Informat Syst, Sydney, NSW, Australia. RP Dow, JM (reprint author), ESA ESOC, Darmstadt, Germany. EM john.dow@esa.int NR 1 TC 14 Z9 14 U1 0 U2 6 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0949-7714 J9 J GEODESY JI J. Geodesy PD JUL PY 2009 VL 83 IS 7 BP 689 EP 689 DI 10.1007/s00190-009-0315-4 PG 1 WC Geochemistry & Geophysics; Remote Sensing SC Geochemistry & Geophysics; Remote Sensing GA 460WP UT WOS:000267222700007 ER PT J AU Kierulf, HP Pettersen, BR MacMillan, DS Willis, P AF Kierulf, Halfdan Pascal Pettersen, Bjorn Ragnvald MacMillan, Daniel S. Willis, Pascal TI The kinematics of Ny-Alesund from space geodetic data SO JOURNAL OF GEODYNAMICS LA English DT Article DE Ny-Alesund; VLBI; GPS; DORIS; Tide gauge; Reference frame ID OBSERVING SYSTEM; PLATE MOTIONS; SEA-LEVEL; DORIS; SERVICE; SVALBARD; TIME; NETWORK AB We have compared coordinate time series from several space geodetic observing techniques to derive the kinematical motions of Ny-Alesund, Svalbard. Velocity estimates from VLBI, GPS, and DORIS scatter more than the expected error estimates from each technique, and also between individual GPS solutions with different software and analysis strategies. A statistical combination yields average topocentric velocity components of 14.3 +/- 0.2 mm/year (north), 9.8 +/- 0.7 mm/year (east), and 8.2 +/- 0.9 mm/year (vertical) for 1993-2007. The horizontal velocity is in agreement with a combined prediction of NUVEL-NNR-1A and the effects of post-glacial rebound and present day ice melt of nearby glaciers. The observed uplift is twice that predicted by the two latter processes. The non-linear time series of both VLBI and GPS data suggest that the uplift rate increases from 7.0 mm/year before 2003 to 10.8 mm/year after 2003. We conclude that this has a geophysical origin since no monument motions have been detected. A recent sea level decrease (1993-2007) of 4.7 +/- 0.9 mm/year supports an absolute sea level increase of 3.2 mm/year as determined elsewhere by satellite altimetry. (C) 2009 Elsevier Ltd. All rights reserved. C1 [Kierulf, Halfdan Pascal] Geodet Inst, Norwegian Mapping Author, N-3507 Honefoss, Norway. [Kierulf, Halfdan Pascal] Univ Oslo, Dept Geosci, N-0316 Oslo, Norway. [Pettersen, Bjorn Ragnvald] Univ Environm & Life Sci, Dept Math Sci & Technol, N-1432 As, Norway. [MacMillan, Daniel S.] NASA, Goddard Space Flight Ctr, NVI Inc, Greenbelt, MD 20771 USA. [Willis, Pascal] Inst Geog Natl, St Mande, France. [Willis, Pascal] Inst Phys Globe, Paris, France. RP Kierulf, HP (reprint author), Geodet Inst, Norwegian Mapping Author, N-3507 Honefoss, Norway. EM halfdan.kierulf@statkart.no RI Willis, Pascal/A-8046-2008 OI Willis, Pascal/0000-0002-3257-0679 FU Research Council of Norway; Centre National d'Etudes Spatial (CNES) in France; IPGP [2498]; [ES0701] FX We are obliged to several staff members of NMA for information on instrument changes and construction work at the Geodetic Observatory in Ny-Alesund, and for collecting and processing the leveling data. Part of this work was supported by the Research Council of Norway, Centre National d'Etudes Spatial (CNES) in France and by COST Action ES0701 "Improved constrains on models of Glacial Isostatic Adjustment". This paper is IPGP contribution 2498. NR 47 TC 19 Z9 19 U1 1 U2 2 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0264-3707 J9 J GEODYN JI J. Geodyn. PD JUL PY 2009 VL 48 IS 1 BP 37 EP 46 DI 10.1016/j.jog.2009.05.002 PG 10 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 465FJ UT WOS:000267567500005 ER PT J AU Satyaprakash, AK Tremaine, AM Stelter, AA Creed, R Ravanfar, P Mendoza, N Mehta, SK Rady, PL Pierson, DL Tyring, SK AF Satyaprakash, Anita K. Tremaine, Anne Marie Stelter, Arwen A. Creed, Rosella Ravanfar, Parisa Mendoza, Natalia Mehta, Satish K. Rady, Peter L. Pierson, Duane L. Tyring, Stephen K. TI Viremia in Acute Herpes Zoster SO JOURNAL OF INFECTIOUS DISEASES LA English DT Article; Proceedings Paper CT 65th Annual Meeting of the American-Academy-of-Dermatology CY FEB 02-06, 2007 CL Washington, DC SP Amer Acad Dermatol ID HUMAN TRIGEMINAL GANGLIA; VIRUS-INFECTION; DIHYDROPYRIMIDINE DEHYDROGENASE; VISCERAL VARICELLA; NATURAL-HISTORY; SORIVUDINE; DNA; CELLS; PCR; QUANTIFICATION AB Background. A phase 2 trial was conducted to evaluate the efficacy of a topical antiviral, sorivudine, as an adjuvant to valacyclovir for the treatment of acute herpes zoster. Methods. In this randomized, placebo-controlled, double-blind trial, 25 patients were treated with either sorivudine or placebo cream. All patients began 7 days of valacyclovir treatment on day 3. Zoster lesion swab samples and samples of peripheral blood mononuclear cells were collected periodically throughout the study and were analyzed for varicella-zoster virus (VZV) DNA by use of both qualitative and real-time polymerase chain reaction. Serum samples collected periodically throughout the study were analyzed for VZV DNA by use of real-time polymerase chain reaction. Results. VZV DNA was detected in all 3 sample types, and the number of viral copies correlated with the progression of herpes zoster. No statistically significant differences were seen between the placebo- and sorivudine-treated groups with respect to clinical characteristics or laboratory test results. Conclusion. The detection of VZV DNA in the serum and peripheral blood mononuclear cells of all 25 zoster patients documents that viremia is a common manifestation of herpes zoster. Sorivudine cream appears to be a safe and well-tolerated adjuvant therapy; however, further phase 2 studies are needed to determine its clinical efficacy for the treatment of herpes zoster. C1 [Satyaprakash, Anita K.; Tremaine, Anne Marie; Stelter, Arwen A.; Creed, Rosella; Ravanfar, Parisa; Mendoza, Natalia; Tyring, Stephen K.] Univ Texas Hlth Sci Ctr, Ctr Clin Studies, Houston, TX USA. [Mehta, Satish K.] Univ Texas Hlth Sci Ctr, Enterprise Advisory Serv, Houston, TX USA. [Pierson, Duane L.] Univ Texas Hlth Sci Ctr, Lyndon B Johnson Space Ctr, NASA, Houston, TX USA. [Rady, Peter L.; Tyring, Stephen K.] Univ Texas Hlth Sci Ctr, Dept Dermatol, Houston, TX USA. [Mendoza, Natalia] Univ El Bosque, Bogota, Colombia. RP Tyring, SK (reprint author), 451 N Texas Ave, Webster, TX 77598 USA. EM styring@ccstexas.com NR 38 TC 10 Z9 10 U1 0 U2 1 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 JUL 1 PY 2009 VL 200 IS 1 BP 26 EP 32 DI 10.1086/599381 PG 7 WC Immunology; Infectious Diseases; Microbiology SC Immunology; Infectious Diseases; Microbiology GA 452CG UT WOS:000266516700006 PM 19469706 ER PT J AU Nyeo, SL Ansari, RR AF Nyeo, Su-Long Ansari, Rafat R. TI EARLY CATARACT DETECTION BY DYNAMIC LIGHT SCATTERING WITH SPARSE BAYESIAN LEARNING SO JOURNAL OF INNOVATIVE OPTICAL HEALTH SCIENCES LA English DT Article DE Cataract; dynamic light scattering; diagnostic algorithm; sparse Bayesian learning (SBL) AB Dynamic light scattering (DLS) is a promising technique for early cataract detection and for studying cataractogenesis. A novel probabilistic analysis tool, the sparse Bayesian learning (SBL) algorithm, is described for reconstructing the most-probable size distribution of alpha-crystallin and their aggregates in an ocular lens from the DLS data. The performance of the algorithm is evaluated by analyzing simulated correlation data from known distributions and DLS data from the ocular lenses of a fetal calf, a Rhesus monkey, and a man, so as to establish the required efficiency of the SBL algorithm for clinical studies. C1 [Nyeo, Su-Long] Natl Cheng Kung Univ, Dept Phys, Tainan 701, Taiwan. [Ansari, Rafat R.] NASA Glenn Res Ctr Lewis Field, Biosci & Technol Branch, Cleveland, OH 44135 USA. RP Nyeo, SL (reprint author), Natl Cheng Kung Univ, Dept Phys, Tainan 701, Taiwan. EM t14269@mail.ncku.edu.tw; Rafat.R.Ansari@nasa.gov FU National Science Council of the Republic of China [NSC-97-2112-M-006-006] FX Part of this work was carried out at the School of Health Information Sciences of the University of Texas Health Science Center at Houston while Dr Nyeo was a visiting Professor and Dr Ansari was a full Professor at UTHSC. The authors are very grateful to Dr J. S. Zigler Jr. for providing the lens samples. Dr Nyeo would like to acknowledge the financial support from the National Science Council of the Republic of China under the Contract No. NSC-97-2112-M-006-006. NR 32 TC 3 Z9 3 U1 0 U2 1 PU WORLD SCIENTIFIC PUBL CO PTE LTD PI SINGAPORE PA 5 TOH TUCK LINK, SINGAPORE 596224, SINGAPORE SN 1793-5458 J9 J INNOV OPT HEAL SCI JI J. Innov. Opt. Health Sci. PD JUL PY 2009 VL 2 IS 3 BP 303 EP 313 DI 10.1142/S1793545809000632 PG 11 WC Optics; Radiology, Nuclear Medicine & Medical Imaging SC Optics; Radiology, Nuclear Medicine & Medical Imaging GA V27YB UT WOS:000208647400012 ER PT J AU Ramesham, R Kullberg, RC AF Ramesham, Rajeshuni Kullberg, Richard C. TI Review of vacuum packaging and maintenance of MEMS and the use of getters therein SO JOURNAL OF MICRO-NANOLITHOGRAPHY MEMS AND MOEMS LA English DT Article DE getters; nonevaporable; evaporable; MEMS packaging; hermetic sealing; vacuum packaging; adsorption; desorption; outgassing ID ACTIVATION; ALLOYS AB Key types of microelectromechanical systems (MEMS) sensors need vacuum or other controlled ambients in order to operate properly. Examples include MEMS infrared sensors and sensitive MEMS gyros. Steps to attain and maintain the vacuum ambient include: (i) Proper processing to reduce trapped gasses in the package, (ii) hermetically sealing the package, and (iii) providing a means to pump away gasses that outgas into the package. Proper package processing and getter technology are key to success in this endeavor. Although many aspects of package processing and assembly are proprietary, the key items to control include leaks (i.e., obtaining a hermetic package) and outgassing from materials within the vacuum cavity. Once gas loads are minimized as much as possible, the actual service life of a package depends on pumping away any internal gases built up through outgassing, leaks, or permeation. This pumping is done by a class of materials called getters. Gettering technology is discussed in relation to vacuum-packaged MEMS/MOEMS. With proper materials and processes, controlled ambients to include vacuum can be obtained in MEMS/MOEMS packages. Not only can they be obtained, they can be maintained for the desired system lifetime. (C) 2009 Society of Photo-Optical Instrumentation Engineers. [DOI: 10.1117/1.3158064] C1 [Ramesham, Rajeshuni] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Kullberg, Richard C.] Arthur Jonath Associates, Portola Valley, CA 94028 USA. RP Ramesham, R (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr,M-S 125-204D, Pasadena, CA 91109 USA. EM Rajeshuni.ramesham@jpl.nasa.gov FU National Aeronautics and Space Administration FX This publication was supported, in part, by the JPL, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. This publication was begun while one of the authors (R.C.K.) was employed by SAES Getters USA, Inc., Colorado Springs, Colorado. The authors thank SAES Getters for the use of certain images and graphs in this paper. NR 27 TC 11 Z9 11 U1 2 U2 20 PU SPIE-SOC PHOTO-OPTICAL INSTRUMENTATION ENGINEERS PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98225 USA SN 1932-5150 EI 1932-5134 J9 J MICRO-NANOLITH MEM JI J. Micro-Nanolithogr. MEMS MOEMS PD JUL-SEP PY 2009 VL 8 IS 3 AR 031307 DI 10.1117/1.3158064 PG 9 WC Engineering, Electrical & Electronic; Nanoscience & Nanotechnology; Materials Science, Multidisciplinary; Optics SC Engineering; Science & Technology - Other Topics; Materials Science; Optics GA 507UY UT WOS:000270881800009 ER PT J AU Ramesham, R Hartzell, AL AF Ramesham, Rajeshuni Hartzell, Allyson L. TI RELIABILITY, PACKAGING, TESTING, AND CHARACTERIZATION OF MEMS AND MOEMS SO JOURNAL OF MICRO-NANOLITHOGRAPHY MEMS AND MOEMS LA English DT Editorial Material C1 [Ramesham, Rajeshuni] NASA, JPL Caltech, Washington, DC 20546 USA. [Hartzell, Allyson L.] Boston Micromachines Corp, Boston, MA USA. RP Ramesham, R (reprint author), NASA, JPL Caltech, Washington, DC 20546 USA. NR 0 TC 0 Z9 0 U1 0 U2 1 PU SPIE-SOC PHOTOPTICAL INSTRUMENTATION ENGINEERS PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98225 USA SN 1537-1646 J9 J MICRO-NANOLITH MEM JI J. Micro-Nanolithogr. MEMS MOEMS PD JUL-SEP PY 2009 VL 8 IS 3 AR 031301 PG 1 WC Engineering, Electrical & Electronic; Nanoscience & Nanotechnology; Materials Science, Multidisciplinary; Optics SC Engineering; Science & Technology - Other Topics; Materials Science; Optics GA 507UY UT WOS:000270881800003 ER PT J AU Nikitin, AV Champion, JP Butler, RAH Brown, LR Kleiner, I AF Nikitin, A. V. Champion, J. -P. Butler, R. A. H. Brown, L. R. Kleiner, I. TI Global modeling of the lower three polyads of PH3: Preliminary results SO JOURNAL OF MOLECULAR SPECTROSCOPY LA English DT Article; Proceedings Paper CT 20th International Conference on High Resolution Molecular Spectroscopy CY SEP 02-06, 2008 CL Prague, CZECH REPUBLIC DE Phosphine; PH3; Vibrational polyads; Global modeling; Near infrared; High-resolution; Positions; Intensities ID ELECTRONIC GROUND-STATE; MU-M; INFRARED-SPECTRUM; SPECTROSCOPIC DATABASE; ROVIBRATIONAL SPECTRA; POLYATOMIC-MOLECULES; (CH3)-C-12 CL-37; PHOSPHINE PH3; DIPOLE-MOMENT; CM(-1) AB In order to model the high-resolution infrared spectrum of the phosphine molecule in the 3 mu m region, a global approach involving the lower three polyads of the molecule (Dyad, Pentad and Octad) as been applied using an effective hamiltonian in the form of irreducible tensors. This model allowed to describe all the 15 vibrational states involved and to consider explicitly all relevant ro-vibrational interactions that cannot be accounted for by conventional perturbation approaches. 2245 levels (up to J = 14) observed through transitions arising from 34 cold and hot bands including all available existing data as well as new experimental data have been fitted simultaneously using a unique set of effective hamiltonian parameters. The rms achieved is 0.63 x 10(-3) cm(-1) for 450 Dyad levels, 1.5 x 10(-3) cm(-1) for 1058 Pentad levels (from 3585 transitions) and 4.3 x 10(-3) cm(-1) for 737 Octad levels (from 2243 transitions). This work represents the first theoretical modeling of the 3 mu m region. It also improves the modeling of the region around 4.5 mu m by dividing the rms reported by previous works by a factor 6. A preliminary intensity analysis based on consistent sets of effective dipole moment operators for cold and hot bands has been simultaneously undertaken for direct comparison between observed and modeled absorption from 700 to 3500 cm(-1). (C) 2009 Elsevier Inc. All rights reserved. C1 [Champion, J. -P.] Univ Bourgogne, CNRS, Inst Carnot Bourgogne, UMR 5209, F-21078 Dijon, France. [Nikitin, A. V.] Russian Acad Sci, Inst Atmospher Opt, Lab Theoret Spect, Tomsk 634055, Russia. [Butler, R. A. H.] Pittsburg State Univ, Pittsburg, KS 66762 USA. [Brown, L. R.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Kleiner, I.] Univ Paris 07, CNRS, Lab Interuniv Syst Atmospher, F-94010 Creteil, France. [Kleiner, I.] Univ Paris 12, CNRS, Lab Interuniv Syst Atmospher, F-94010 Creteil, France. RP Champion, JP (reprint author), Univ Bourgogne, CNRS, Inst Carnot Bourgogne, UMR 5209, 9 Av A Savary,BP 47870, F-21078 Dijon, France. EM jean-paul.champion@u-bourgogne.fr RI Champion, Jean-Paul/C-3963-2009; Nikitin, Andrei/K-2624-2013 OI Nikitin, Andrei/0000-0002-4280-4096 NR 31 TC 11 Z9 11 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 0022-2852 J9 J MOL SPECTROSC JI J. Mol. Spectrosc. PD JUL PY 2009 VL 256 IS 1 SI SI BP 4 EP 16 DI 10.1016/j.jms.2009.01.008 PG 13 WC Physics, Atomic, Molecular & Chemical; Spectroscopy SC Physics; Spectroscopy GA 475XO UT WOS:000268400600002 ER PT J AU Kenny, RJ Hulka, JR Moser, MD Rhys, NO AF Kenny, R. J. Hulka, James R. Moser, Marlow D. Rhys, Noah O. TI Effect of Chamber Backpressure on Swirl Injector Fluid Mechanics SO JOURNAL OF PROPULSION AND POWER LA English DT Article AB Fluid mechanics of a liquid swirl injector element at various chamber backpressures were investigated. The center-jet swirling element was designed using typical liquid propellant rocket engine parameters, then manufactured and tested in a high-pressure, optically accessible, cold flow facility. Water was injected into a chamber pressurized with gaseous nitrogen at a constant swirl injector How rate of 0.09 kg/s. The chamber backpressure ranged from 0.10 to 4.81 MPa. The film thickness and spray angle near the nozzle exit were measured by shadowgraphy. The film thickness was also measured within the injector upstream of the exit through a transparent nozzle tube section. Increasing the chamber backpressure for this fixed mass How rate increased the film thickness from predicted design values. Measured discharge coefficient values increased with increasing chamber backpressure, reflecting the observed increase in internal nozzle film thickness. The spray angle decreased for increasing chamber backpressure. C1 [Kenny, R. J.] NASA, George C Marshall Space Flight Ctr, Acoust & Stabil Team, Huntsville, AL 35812 USA. [Hulka, James R.] Jacobs Engn, Engn Sci & Tech Serv Grp, Huntsville, AL 35812 USA. [Moser, Marlow D.] Univ Alabama, Dept Mech & Aerosp Engn, Huntsville, AL 35812 USA. [Rhys, Noah O.] Yetispace Inc, Huntsville, AL 35802 USA. RP Kenny, RJ (reprint author), NASA, George C Marshall Space Flight Ctr, Acoust & Stabil Team, Mail Stop ER42, Huntsville, AL 35812 USA. FU NASA's Constellation University Institutes Project FX This work was funded under NASA's Constellation University Institutes Project, directed by Claudia Meyer and Jeff Rybak. Facility support was reliably provided by the personnel of NASA Marshall Space Flight Center's East Test Area. Nick Hensley provided excellent support during testing. NR 18 TC 15 Z9 16 U1 2 U2 7 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 JUL-AUG PY 2009 VL 25 IS 4 BP 902 EP 913 DI 10.2514/1.38537 PG 12 WC Engineering, Aerospace SC Engineering GA 473KI UT WOS:000268204500007 ER PT J AU Almini, AA Kulahci, M Montgomery, DC AF Almini, Ashraf A. Kulahci, Murat Montgomery, Douglas C. TI Checking the Adequacy of Fit of Models from Split-Plot Designs SO JOURNAL OF QUALITY TECHNOLOGY LA English DT Article DE Model Adequacy Checking; PRESS; Residual Analysis; R(2); R(2)-Adjusted; R(2)-Prediction; Subplot Error; Whole-Plot Error ID COEFFICIENT; PREDICTION AB One of the main features that distinguish split-plot experiments from other experiments is that they involve two types of experimental errors: the whole-plot (WP) error and the subplot (SP) error. Taking this into consideration is very important when computing measures of adequacy of fit for split-plot models. In this article, we propose the computation of two R(2), R(2)-adjusted, prediction error sums of squares (PRESS), and R(2)-prediction statistics to measure the adequacy of fit for the WP and the SP submodels in a split-plot design. This is complemented with the graphical analysis of the two types of errors to check for any violation of the underlying assumptions and the adequacy of fit of split-plot models. Using examples, we show how computing two measures of model adequacy of fit for each split-plot design model is appropriate and useful as they reveal whether the correct WP and SP effects have been included in the model and describe the predictive performance of each group of effects. C1 [Almini, Ashraf A.] NASA, Langley Res Ctr, Hampton, VA 23681 USA. [Kulahci, Murat] Tech Univ Denmark, Dept Informat & Math Modeling, DK-2800 Lyngby, Denmark. [Montgomery, Douglas C.] Arizona State Univ, Dept Ind Syst & Operat Engn, Tempe, AZ 85287 USA. RP Almini, AA (reprint author), NASA, Langley Res Ctr, Hampton, VA 23681 USA. EM Ashrafalmini@gmail.com; mk@imm.dtu.dk; doug.montgomery@asu.edu OI kulahci, murat/0000-0003-4222-9631 FU Fulbright Foreign Student Exchange Program; United States Department of State FX The authors would like to thank the editor and two anonymous referees for their valuable comments. Almimi's work was supported by the Fulbright Foreign Student Exchange Program, which is administered by AMIDEAST and funded by the United States Department of State. NR 25 TC 2 Z9 2 U1 0 U2 0 PU AMER SOC QUALITY CONTROL-ASQC PI MILWAUKEE PA 600 N PLANKINTON AVE, MILWAUKEE, WI 53203 USA SN 0022-4065 J9 J QUAL TECHNOL JI J. Qual. Technol. PD JUL PY 2009 VL 41 IS 3 BP 272 EP 284 PG 13 WC Engineering, Industrial; Operations Research & Management Science; Statistics & Probability SC Engineering; Operations Research & Management Science; Mathematics GA 464LV UT WOS:000267507300006 ER PT J AU Mishchenko, MI AF Mishchenko, Michael I. TI Electromagnetic scattering by nonspherical particles: A tutorial review SO JOURNAL OF QUANTITATIVE SPECTROSCOPY & RADIATIVE TRANSFER LA English DT Article; Proceedings Paper CT Annual Meeting of the Association-for-Aerosol-Research CY JUL 03-04, 2008 CL Karlsruhe, GERMANY SP Assoc Aerosol Res DE Electromagnetic scattering; Nonspherical particles; Polarization ID RADIATIVE-TRANSFER EQUATION; DISCRETE RANDOM MEDIUM; SMALL ICE CRYSTALS; LIGHT-SCATTERING; MULTIPLE-SCATTERING; ABSORBING MEDIUM; SPECIAL-ISSUE; POLARIZED-LIGHT; T-MATRIX; COHERENT BACKSCATTERING AB This tutorial review is intended to provide an accessible and self-contained introduction to the discipline of electromagnetic scattering by nonspherical particles and discuss the most general ways in which the scattering and absorption properties of particles and small random particle groups are affected by particle morphology. The main focus is on how nonsphericity influences our way of describing and quantifying electromagnetic scattering by particles and how it is likely to affect, both qualitatively and quantitatively, the principal theoretical descriptors of scattering and the relevant optical observables. Several quantitative examples included in this review are the result of a controlled laboratory measurement or a numerically exact theoretical computation and are intended to illustrate the main theses and conclusions. Published by Elsevier Ltd. C1 NASA, Goddard Inst Space Studies, New York, NY 10025 USA. RP Mishchenko, MI (reprint author), NASA, Goddard Inst Space Studies, 2880 Broadway, New York, NY 10025 USA. EM mmishchenko@giss.nasa.gov RI Mishchenko, Michael/D-4426-2012 NR 141 TC 46 Z9 46 U1 1 U2 15 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 JUL PY 2009 VL 110 IS 11 SI SI BP 808 EP 832 DI 10.1016/j.jqsrt.2008.12.005 PG 25 WC Optics; Spectroscopy SC Optics; Spectroscopy GA 459EB UT WOS:000267082200004 ER PT J AU Berger, KT AF Berger, Karen T. TI Aerothermodynamic Testing of the Crew Exploration Vehicle at Mach 6 and Mach 10 SO JOURNAL OF SPACECRAFT AND ROCKETS LA English DT Article; Proceedings Paper CT AIAA 46th Aerospace Sciences Meeting and Exhibit CY JAN 07-10, 2008 CL Reno, NV SP Amer Inst Aeronaut & Astronaut AB An experimental wind-tunnel program is being conducted in support of a NASA wide effort to develop a Space Shuttle replacement and to support the agency's long-term objective of returning to the moon and Mars. This paper documents experimental measurements made on several scaled ceramic heat transfer models of the proposed Project Orion Crew Exploration Vehicle. The experimental data highlighted in this paper will be used to assess numerical tools that will be used to generate the flight aerothermodynamic database. Global heat transfer images and centerline heat transfer distributions were obtained over a range of freestream Reynolds numbers and angles of attack with the phosphor thermography technique. Temperature data were measured on the forebody and afterbody and were used to compute the heating on the vehicle as well as the boundary-layer state on the forebody surface. Several model support configurations were assessed to minimize potential aftbody support interference. Although naturally fully developed turbulent levels were not obtained on the forebody, the use of boundary-layer trips generated fully developed turbulent flow. Laminar and turbulent computational results are shown to be in good agreement with the data. In addition, the ability of the global phosphor thermography method to provide quantitative heating measurements in the low-temperature environment of the capsule base region was assessed and the lack of significant model support hardware influence on heating was shown. C1 NASA, Langley Res Ctr, Aerothermodynam Branch, Hampton, VA 23681 USA. RP Berger, KT (reprint author), NASA, Langley Res Ctr, Aerothermodynam Branch, Mail Stop 408A, Hampton, VA 23681 USA. NR 9 TC 4 Z9 4 U1 0 U2 1 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 JUL-AUG PY 2009 VL 46 IS 4 BP 758 EP 765 DI 10.2514/1.39247 PG 8 WC Engineering, Aerospace SC Engineering GA 482RT UT WOS:000268907100003 ER PT J AU Hollis, BR Berger, KT Horvath, TJ Coblish, JJ Norris, JD Lillard, RP Kirk, BS AF Hollis, Brian R. Berger, Karen T. Horvath, Thomas J. Coblish, Joseph J. Norris, Joseph D. Lillard, Randolph P. Kirk, Benjamin S. TI Aeroheating Testing and Predictions for Project Orion Crew Exploration Vehicle SO JOURNAL OF SPACECRAFT AND ROCKETS LA English DT Article; Proceedings Paper CT AIAA 46th Aerospace Sciences Meeting and Exhibit CY JAN 07-10, 2008 CL Reno, NV SP Amer Inst Aeronaut & Astronaut ID TRANSITION; SCHEMES AB An investigation of the aeroheating environment of the Project Orion Crew Exploration Vehicle was performed in the Arnold Engineering Development Center Hypervelocity Wind Tunnel 9 Mach 8 and Mach 10 nozzles and in the NASA Langley Research Center 20-Inch Mach 6 Air Tunnel. Heating data were obtained using a thermocouple-instrumented similar to 0.035-scale model [0.1778 m (7 in.) diameter] of the flight vehicle. Runs were performed in the Tunnel 9 Mach 10 nozzle at freestream unit Reynolds numbers of 1 x 10(6) to 20 x 10(6)/ft, in the Tunnel 9 Mach 8 nozzle at freestream unit Reynolds numbers of 8 x 10(6) to 48 x 10(6)/ft, and in the 20-Inch Mach 6 Air Tunnel at freestream unit Reynolds numbers of 1 x 10(6) to 7 x 10(6)/ft. In both facilities, enthalpy levels were low and the test gas (N(2) in Tunnel 9 and air in the 20-Inch Mach 6 Air Tunnel) behaved as a perfect gas. These test conditions produced laminar, transitional, and turbulent data in the Tunnel 9 Mach 10 nozzle; transitional and turbulent data in the Tunnel 9 Mach 8 nozzle; and laminar and transitional data in the 20-Inch Mach 6 Air Tunnel. Laminar and turbulent predictions were generated for all wind-tunnel test conditions, and comparisons were performed with the experimental data to help define the accuracy of the computational method. In general, it was found that both laminar data and predictions and turbulent data and predictions agreed to within less than the estimated +/- 12% experimental uncertainty estimate. Laminar heating distributions from all three data sets were shown to correlate well and demonstrated Reynolds numbers independence when expressed in terms of the Stanton number based on adiabatic-wall-recovery enthalpy. Transition-onset locations on the lee-side centerline were determined from the data and correlated in terms of boundary-layer parameters. Finally, turbulent heating augmentation ratios were determined for several body-point locations and correlated in terms of the boundary-layer momentum Reynolds number. C1 [Hollis, Brian R.; Berger, Karen T.; Horvath, Thomas J.] NASA, Langley Res Ctr, Aerothermodynam Branch, Hampton, VA 23681 USA. [Coblish, Joseph J.; Norris, Joseph D.] Arnold Engn Dev Ctr, White Oak, MD 20901 USA. [Lillard, Randolph P.; Kirk, Benjamin S.] NASA, Lyndon B Johnson Space Ctr, Appl Aerosci & CFD Branch, Houston, TX 77058 USA. RP Hollis, BR (reprint author), NASA, Langley Res Ctr, Aerothermodynam Branch, Hampton, VA 23681 USA. NR 28 TC 6 Z9 6 U1 0 U2 1 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 JUL-AUG PY 2009 VL 46 IS 4 BP 766 EP 780 DI 10.2514/1.38579 PG 15 WC Engineering, Aerospace SC Engineering GA 482RT UT WOS:000268907100004 ER PT J AU Murman, SM AF Murman, Scott M. TI Dynamic Simulations of Atmospheric-Entry Capsules SO JOURNAL OF SPACECRAFT AND ROCKETS LA English DT Article; Proceedings Paper CT 26th AIAA Applied Aerodynamics Conference CY AUG 18-21, 2008 CL Honolulu, HI SP AIAA ID TRANSONIC SPEEDS; REENTRY CAPSULE; STABILITY AB Viscous free-oscillation simulations with the OVERFLOW solver are used to predict the aerodynamic behavior of nonlifting capsule shapes in the supersonic-speed regime. Computations using hybrid Reynolds-averaged Navier-Stokes turbulence models are examined for two novel atmospheric-entry capsule configurations: an idealized inflatable decelerator concept and the Orion crew module. The simulation results are validated against nonlinear aerodynamic models determined from free-flight ballistic-range data analysis. For the Orion crew module, two separate methods of reducing identical range data, along with common models tested in separate range facilities, are included. The computations demonstrate the efficiency and accuracy of dynamic simulations for developing a nonlinear aerodynamic performance database. Analysis indicates that the typical nonlinear bluff-body behavior is characterized by a rate-dependent dynamic response, which is not currently accounted for in common aerodynamic models. C1 NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Murman, SM (reprint author), NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. EM Scott.M.Murman@nasa.gov NR 28 TC 3 Z9 4 U1 2 U2 5 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 JUL-AUG PY 2009 VL 46 IS 4 BP 829 EP 835 DI 10.2514/1.41078 PG 7 WC Engineering, Aerospace SC Engineering GA 482RT UT WOS:000268907100010 ER PT J AU Al-Hamdan, MZ Crosson, WL Limaye, AS Rickman, DL Quattrochi, DA Estes, MG Qualters, JR Sinclair, AH Tolsma, DD Adeniyi, KA Niskar, AS AF Al-Hamdan, Mohammad Z. Crosson, William L. Limaye, Ashutosh S. Rickman, Douglas L. Quattrochi, Dale A. Estes, Maurice G., Jr. Qualters, Judith R. Sinclair, Amber H. Tolsma, Dennis D. Adeniyi, Kafayat A. Niskar, Amanda Sue TI Methods for Characterizing Fine Particulate Matter Using Ground Observations and Remotely Sensed Data: Potential Use for Environmental Public Health Surveillance SO JOURNAL OF THE AIR & WASTE MANAGEMENT ASSOCIATION LA English DT Article ID AEROSOL OPTICAL-THICKNESS; DISTANCE WEIGHTED INTERPOLATION; AIR-QUALITY; LEVEL PM2.5; UNITED-STATES; POLLUTION; EXPOSURE; DEPTH; MODIS AB This study describes and demonstrates different techniques for surface-fitting daily environmental hazards data of particulate matter with aerodynamic diameter less than or equal to 2.5 mu m (PM(2.5)) for the purpose of integrating respiratory health and environmental data for the Centers for Disease Control and Prevention (CDC) pilot study of Health and Environment Linked for Information Exchange (HELIX)-Atlanta. It presents a methodology for estimating daily spatial surfaces of ground-level PM(2.5) concentrations using the B-Spline and inverse distance weighting (IDW) surface-fitting techniques, leveraging National Aeronautics and Space Administration (NASA) Moderate Resolution Imaging Spectrometer (MODIS) data to complement U.S. Environmental Protection Agency (EPA) ground observation data. The study used measurements of ambient PM(2.5) from the EPA database for the year 2003 as well as PM(2.5) estimates derived from NASA's satellite data. Hazard data have been processed to derive the surrogate PM(2.5) exposure estimates. This paper shows that merging MODIS remote sensing data with surface observations of PM(2.5) not only provides a more complete daily representation of PM(2.5) than either dataset alone would allow, but it also reduces the errors in the PM(2.5-) estimated surfaces. The results of this study also show that although the IDW technique can introduce some numerical artifacts that could be due to its interpolating nature, which assumes that the maxima and minima can occur only at the observation points, the daily IDW PM,., surfaces had smaller errors in general, with respect to observations, than those of the B-Spline surfaces. Finally, the methods discussed in this paper establish a foundation for environmental public health linkage and association studies for which determining the concentrations of an environmental hazard such as PM(2.5) with high accuracy is critical. C1 [Al-Hamdan, Mohammad Z.; Crosson, William L.; Limaye, Ashutosh S.; Estes, Maurice G., Jr.] NASA, George C Marshall Space Flight Ctr, Univ Space Res Assoc, Natl Space Sci & Technol Ctr,Global Hydrol & Clim, Huntsville, AL 35805 USA. [Rickman, Douglas L.; Quattrochi, Dale A.] NASA, George C Marshall Space Flight Ctr, Earth Sci Off, Natl Space Sci & Technol Ctr,Global Hydrol & Clim, Huntsville, AL 35805 USA. [Qualters, Judith R.] Ctr Dis Control & Prevent, Environm Hlth Tracking Branch, Div Environm Hazards & Hlth Effects, Natl Ctr Environm Hlth, Atlanta, GA USA. [Sinclair, Amber H.; Tolsma, Dennis D.] Ctr Hlth Res SE Kaiser Permanente, Atlanta, GA USA. [Adeniyi, Kafayat A.] Northrop Grumman, Atlanta, GA USA. [Niskar, Amanda Sue] US Dept HHS, Off Assistant Secretary Preparedness & Response, Off Preparedness & Emergency Operat, Fus Cell, Washington, DC 20201 USA. RP Al-Hamdan, MZ (reprint author), NASA, George C Marshall Space Flight Ctr, Univ Space Res Assoc, Natl Space Sci & Technol Ctr,Global Hydrol & Clim, 320 Sparkman Dr, Huntsville, AL 35805 USA. EM mohammad.alhamdan@nasa.gov OI Tolsma, Dennis/0000-0002-0685-0618; Rickman, Doug/0000-0003-3409-2882 FU NASA; CDC National Environmental Public Health Tracking Program; HELIX-Atlanta Partners FX The authors acknowledge the generous support of the NASA Applied Sciences Public Health Program, CDC National Environmental Public Health Tracking Program, and HELIX-Atlanta Partners. The authors also thank Darren Palmer from EPA for providing AQS data and assistance in using it; Dr. Jeremy Sarnat from Emory University for helpful comments on the manuscript; and Sue Estes from USRA at NASA/MSFC and Diane Samuelson from the Earth Science Office at NASA/MSFC for invaluable editing assistance. Finally, the authors thank the editor of this journal and three anonymous reviewers for their helpful comments and suggestions. NR 34 TC 18 Z9 18 U1 0 U2 5 PU AIR & WASTE MANAGEMENT ASSOC PI PITTSBURGH PA ONE GATEWAY CENTER, THIRD FL, PITTSBURGH, PA 15222 USA SN 1047-3289 J9 J AIR WASTE MANAGE JI J. Air Waste Manage. Assoc. PD JUL PY 2009 VL 59 IS 7 BP 865 EP 881 DI 10.3155/1047-3289.59.7.865 PG 17 WC Engineering, Environmental; Environmental Sciences; Meteorology & Atmospheric Sciences SC Engineering; Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences GA 466QC UT WOS:000267676200010 PM 19645271 ER PT J AU Cicolani, LS Cone, A Theron, JN Robinson, LTCD Lusardi, J Tischler, MB Rosen, A Raz, R AF Cicolani, Luigi S. Cone, Andrew Theron, Johannes N. Robinson, L. T. C. Dwight Lusardi, Jeffery Tischler, Mark B. Rosen, Aviv Raz, Reuben TI Flight Test and Simulation of a Cargo Container Slung Load in Forward Flight SO JOURNAL OF THE AMERICAN HELICOPTER SOCIETY LA English DT Article AB This paper presents recent results from a cooperative effort by the U.S. Army Aeroflightdynamics Directorate, the Technion Israel Institute of Technology, and Northern Arizona University to study and simulate the behavior of the 6 x 6 x 8 ft CONEX cargo container in forward flight suspended beneath a UH-60 Black Hawk helicopter. This load, like other cargo containers, is subject to massively separated unsteady flow and is limited by stability to operational airspeeds well below the power-limited speed of the configuration. The study makes use of aerodynamic data from wind tunnel, flight test, and computational fluid dynamics. The objective is a simulation of the helicopter slung load system validated over the complete flight envelope. The principal remaining technical challenge is a model of the unsteady load aerodynamics capable of predicting the critical unstable speed. Some progress has been made in meeting this challenge. C1 [Cicolani, Luigi S.] San Jose State Univ Fdn, Aeroflightdynam Directorate, Moffett Field, CA USA. [Cone, Andrew] Calif Polytech Inst, San Luis Obispo, CA USA. [Theron, Johannes N.] No Arizona Univ, Flagstaff, AZ 86011 USA. [Robinson, L. T. C. Dwight; Lusardi, Jeffery; Tischler, Mark B.] NASA, Ames Res Ctr, US Army Res Dev & Engn Command, Aeroflightdynam Directorate AMRDEC, Moffett Field, CA 94035 USA. [Rosen, Aviv; Raz, Reuben] Technion Israel Inst Technol, Haifa, Israel. RP Cicolani, LS (reprint author), San Jose State Univ Fdn, Aeroflightdynam Directorate, Moffett Field, CA USA. EM luigi.cicolani@us.army.mil NR 31 TC 10 Z9 12 U1 0 U2 1 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 JUL PY 2009 VL 54 IS 3 AR 032006 DI 10.4050/JAHS.54.032006 PG 18 WC Engineering, Aerospace SC Engineering GA V16MR UT WOS:000207874200006 ER PT J AU Lim, JW McAlister, KW Johnson, W AF Lim, Joon W. McAlister, Kenneth W. Johnson, Wayne TI Hover Performance Correlation for Full-Scale and Model-Scale Coaxial Rotors SO JOURNAL OF THE AMERICAN HELICOPTER SOCIETY LA English DT Article ID VORTEX AB The hover performance data of full-scale and model-scale coaxial rotors have been compared with CAMRAD II predictions having a free vortex wake analysis. Performance correlations of a coaxial rotor were made with a variation of key parameters including the rotor spacing and height. To understand aerodynamic behavior of the U.S. Army Aeroflightdynamics Directorate (AFDD) coaxial rotor operating over a range of Reynolds numbers from 36,000 to 180,000, the Reynolds number scaling effect was explored using an airfoil design code, MSES. It was found that the coaxial rotor spacing effect on hover performance was minimal for the rotor spacing larger than 20% of the rotor diameter. The measured performance data showed that more thrust was lost from the lower rotor of a coaxial than the upper rotor due to a larger rotor-to-rotor wake interference effect, and the lower rotor kept only an 81% of the single rotor OGE (out-of-ground effect) thrust whereas the upper rotor maintained a 90%. The lower rotor IGE (in-ground effect) thrust increased quickly by 26% as the rotor approached to the ground from the position of an 80% of the rotor diameter to 10%, and the corresponding IGE power increased by 17%. These thrust and power characteristics were well predicted. Overall, the performance prediction for the coaxial rotor was satisfactory when compared with the measured data. C1 [Lim, Joon W.; McAlister, Kenneth W.] US Army Res Dev & Engn Command, Ames Res Ctr, Aeroflightdynam Directorate AMRDEC, Moffett Field, CA USA. [Johnson, Wayne] NASA, Ames Res Ctr, Aeromech Branch, Moffett Field, CA 94035 USA. RP Lim, JW (reprint author), US Army Res Dev & Engn Command, Ames Res Ctr, Aeroflightdynam Directorate AMRDEC, Moffett Field, CA USA. EM joon.lim@us.army.mil NR 30 TC 7 Z9 7 U1 0 U2 7 PU AMER HELICOPTER SOC INC PI ALEXANDRIA PA 217 N WASHINGTON ST, ALEXANDRIA, VA 22314 USA SN 0002-8711 J9 J AM HELICOPTER SOC JI J. Am. Helicopter Soc. PD JUL PY 2009 VL 54 IS 3 AR 032005 DI 10.4050/JAHS.54.032005 PG 14 WC Engineering, Aerospace SC Engineering GA V16MR UT WOS:000207874200005 ER PT J AU Prahl, SA Fischer, DG Duncan, DD AF Prahl, Scott A. Fischer, David G. Duncan, Donald D. TI Monte Carlo Green's function formalism for the propagation of partially coherent light SO JOURNAL OF THE OPTICAL SOCIETY OF AMERICA A-OPTICS IMAGE SCIENCE AND VISION LA English DT Article ID RAY-BASED SIMULATION; TURBID MEDIA; BEAMS AB We present a Monte Carlo-derived Green's function for the propagation of partially spatially coherent fields. This Green's function, which is derived by sampling Huygens-Fresnel wavelets, can be used to propagate fields through an optical system and to compute first- and second-order field statistics directly. The concept is illustrated for a cylindrical 61 imaging system. A Gaussian copula is used to synthesize realizations of a Gaussian Schell-model field in the pupil plane. Physical optics and Monte Carlo predictions are made for the first- and second-order statistics of the field in the vicinity of the focal plane for a variety of source coherence conditions. Excellent agreement between the physical optics and Monte Carlo predictions is demonstrated in all cases. This formalism can be generally employed to treat the interaction of partially coherent fields with diffracting structures. (C) 2009 Optical Society of America C1 [Prahl, Scott A.] Providence St Vincent Med Ctr, Oregon Med Laser Ctr, Portland, OR 97225 USA. [Fischer, David G.] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. [Duncan, Donald D.] Oregon Hlth & Sci Univ, Div Biomed Engn, Portland, OR 97239 USA. RP Prahl, SA (reprint author), Providence St Vincent Med Ctr, Oregon Med Laser Ctr, 9205 SW Barnes Rd, Portland, OR 97225 USA. EM prahl@bme.ogi.edu FU National Institutes of Health (NIH) [1R21DE016758-01A2] FX Scott Prahl recognizes partial support from National Institutes of Health (NIH), grant 1R21DE016758-01A2. NR 24 TC 8 Z9 8 U1 1 U2 4 PU OPTICAL SOC AMER PI WASHINGTON PA 2010 MASSACHUSETTS AVE NW, WASHINGTON, DC 20036 USA SN 1084-7529 J9 J OPT SOC AM A JI J. Opt. Soc. Am. A-Opt. Image Sci. Vis. PD JUL PY 2009 VL 26 IS 7 BP 1533 EP 1543 PG 11 WC Optics SC Optics GA 476UL UT WOS:000268471500002 PM 19568287 ER PT J AU Selvam, RP Hamilton, MT Johnston, JE Silk, EA AF Selvam, R. Panneer Hamilton, Matthew T. Johnston, Joseph E., III Silk, Eric A. TI Thermal Modeling of Spray Cooling: Gravitational Effect on Droplet and Bubble Dynamics SO JOURNAL OF THERMOPHYSICS AND HEAT TRANSFER LA English DT Article ID HEAT-TRANSFER; NUMERICAL-SIMULATION; PRESSURES; GRAVITY AB As the need for thermal management of high-power density electronic systems on space-based platforms (i.e., laser diode arrays, multichip modules, etc.) grows, interest in spray cooling as a thermal management solution is also increasing. The present study investigates numerically the effects of microgravity and macrogravity on spray cooling heat transfer as well as the effect of droplet impact on vapor bubble growth and development in a liquid film at the heater surface. A two-dimensional, multiphase flow computer model has been developed that includes the effects of surface tension, viscosity, phase change, and gravity. The liquid-vapor interface is modeled using the level set method. Initially, vapor bubble growth is simulated as pool boiling in the film's macroregion (1 to 10 mm normal to the heated wall) for purposes of model verification. Then, bubble merger in a thin film is simulated under microgravity and macrogravity conditions. Finally, droplet impingement is included in the thin-film model, and gravitational effects on the transport properties are discussed. For the thin-film bubble merger and droplet impingement simulation studies, the liquid film adjacent to the heated wall has been approximated as 70 mu m thick. Wall heat transfer during droplet impingement was computed in terms of the nondimensional Nusselt number for gravitational constants ranging from 0.0001 to 2g. Computed Nusselt number versus time is presented and explained using spatial velocity vector diagrams for each simulation case. All of the computational studies were performed using FC-72 as the simulated fluid. C1 [Selvam, R. Panneer; Hamilton, Matthew T.; Johnston, Joseph E., III] Univ Arkansas, Fayetteville, AR 72701 USA. [Silk, Eric A.] NASA, Goddard Space Flight Ctr, Thermal Engn Technol Dev Group, Greenbelt, MD 20771 USA. RP Selvam, RP (reprint author), Univ Arkansas, Bell Engn Ctr 4190, Fayetteville, AR 72701 USA. EM rps@uark.edu RI selvam, Rathinam/H-7849-2013 FU PELS; LLC; University of Arkansas, Fayetteville FX This work was made possible by phase II SBIR grant number NNG06CA07C from NASA Goddard Space Center, Eric Silk contract coordinator, funded through PELS, LLC and the University of Arkansas, Fayetteville. The work was performed at the Computational Mechanics Laboratory at the University of Arkansas, Fayetteville. NR 26 TC 1 Z9 1 U1 2 U2 7 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 JUL-SEP PY 2009 VL 23 IS 3 BP 560 EP 570 DI 10.2514/1.36718 PG 11 WC Thermodynamics; Engineering, Mechanical SC Thermodynamics; Engineering GA 474QY UT WOS:000268300300016 ER PT J AU Elston, LJ Yerkes, KL Thomas, SK McQuillen, J AF Elston, Levi J. Yerkes, Kirk L. Thomas, Scott K. McQuillen, John TI Cooling Performance of a 16-Nozzle Array in Variable Gravity SO JOURNAL OF THERMOPHYSICS AND HEAT TRANSFER LA English DT Article ID HEAT-TRANSFER; SPRAY AB The objective of this paper was to investigate the cooling performance of a 16-nozzle spray array using FC-72 as the working fluid in variable-gravity conditions. A flight-test experiment was modified to accommodate a 16-nozzle spray array, which was then tested in the parabolic flight trajectory environment of NASA's C-9 reduced-gravity aircraft. The 16-nozzle array was designed to cool a 25.4 x 25.4 mm(2) area on a thick-film resistive heater used to simulate an electronic component. Flight tests were conducted over the course of two flight weeks (each week consisting of four flights and each flight consisting of 40 to 60 parabolas). The mass How rate through the 16-nozzle spray array ranged from 13.1 <= (m) over dot <= 21.3 g/s. The heat flux at the thick-film resistor ranged from 2.9 <= q" <= 25 W/cm(2), the subcooling of the working fluid ranged from 1.6 <= Delta T-sc <= 18.4 degrees C, the saturation temperature ranged from 37.4 <= T-sat <= 47.2 degrees C, and the absorbed air content in the working fluid was C = 10.1, 14.3 and 16.8% by volume. The spray chamber pressure ranged from 42 <= P <= 78 kPa and the acceleration ranged from -0.02 <= a <= -2.02 g. Two-phase cooling was emphasized, but some single-phase data were also collected. A one-dimensional model was used to predict the heater surface temperature from the heat input and mean heater base temperature. It was found that the cooling performance was enhanced in microgravity over terrestrial and elevated gravity. In addition, a sudden degradation in performance was found at high mass flow rates in microgravity, possibly due to liquid buildup on the surface between the nozzle impact zones. A high degree of subcooling was found to be beneficial, but the dissolved air content had little effect on the heat transfer performance in either microgravity or elevated gravity. C1 [Elston, Levi J.] USAF, Res Lab, Thermal & Electrochem Branch, Wright Patterson AFB, OH 45433 USA. [Yerkes, Kirk L.] USAF, Res Lab, Energy Power Thermal Div, Wright Patterson AFB, OH 45433 USA. [Thomas, Scott K.] Wright State Univ, Dept Mech & Mat Engn, Dayton, OH 45435 USA. [McQuillen, John] NASA, John H Glenn Res Ctr, Lewis Field, Micrograv Fluid Phys Branch, Cleveland, OH 44135 USA. RP Elston, LJ (reprint author), USAF, Res Lab, Thermal & Electrochem Branch, 1950 5th St,Bldg 18, Wright Patterson AFB, OH 45433 USA. NR 34 TC 3 Z9 3 U1 2 U2 7 PU AMER INST AERONAUTICS ASTRONAUTICS PI RESTON PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA SN 0887-8722 EI 1533-6808 J9 J THERMOPHYS HEAT TR JI J. Thermophys. Heat Transf. PD JUL-SEP PY 2009 VL 23 IS 3 BP 571 EP 581 DI 10.2514/1.41653 PG 11 WC Thermodynamics; Engineering, Mechanical SC Thermodynamics; Engineering GA 474QY UT WOS:000268300300017 ER PT J AU Bonneaud, C Sepil, I Mila, B Buermann, W Pollinger, J Sehgal, RNM Valkiunas, G Iezhova, TA Saatchi, S Smith, TB AF Bonneaud, Camille Sepil, Irem Mila, Borja Buermann, Wolfgang Pollinger, John Sehgal, Ravinder N. M. Valkiunas, Gediminas Iezhova, Tatjana A. Saatchi, Sassan Smith, Thomas B. TI The prevalence of avian Plasmodium is higher in undisturbed tropical forests of Cameroon SO JOURNAL OF TROPICAL ECOLOGY LA English DT Article DE agroforest; Andropadus latirostris; Andropadus virens; Cyanomitra obscura; Haemoproteus; host-parasite interaction; Plasmodium; primary forest; rain-forest birds ID HAEMOPROTEUS-BELOPOLSKYI HAEMOSPORIDA; BLOOD PARASITES; MALARIA PARASITES; LYME-DISEASE; BLUE TITS; BODY-MASS; HOST; BIRDS; RISK; DEFORESTATION AB Habitat fragmentation and deforestation are thought to disrupt host-parasite interactions and increase the risk of epizootic outbreaks in wild vertebrates. A total of 220 individuals from three species of African rain-forest bird (Andropadus latirostris, Andropadus virens, Cyanomitra obscura), captured in two pristine and two agroforests in Cameroon. were screened for the presence of avian haemosporidian parasites (species of Plasmodium and Haemwoproteus) to test whether habitat differences were associated with differences in the prevalence of infectious diseases in natural populations. Thirteen mitochondrial lineages, including 11 Plasmodium and two Haemoproteus lineages were identified. Whereas levels of Haemoproteus spp. infections were too low to permit analysis, the prevalence of infections with Plasmodium spp. reached significantly greater levels in undisturbed mature forests. Importantly however, the significant association between forest type and parasite prevalence was independent of host density effects, suggesting that the association did not reflect changes in host species composition and abundance between forest types. Our results illustrate how characterizing land-cover differences, and hence changes, may be a prerequisite to understanding and predicting patterns of parasite infections in natural populations of rain-forest birds. C1 [Bonneaud, Camille; Sepil, Irem; Buermann, Wolfgang; Pollinger, John; Sehgal, Ravinder N. M.; Saatchi, Sassan; Smith, Thomas B.] Univ Calif Los Angeles, Ctr Trop Res, Inst Environm, Los Angeles, CA 90095 USA. [Mila, Borja; Smith, Thomas B.] Univ Calif Los Angeles, Dept Ecol & Evolutionary Biol, Los Angeles, CA 90095 USA. [Sehgal, Ravinder N. M.] San Francisco State Univ, Dept Biol, San Francisco, CA 94132 USA. [Valkiunas, Gediminas; Iezhova, Tatjana A.] Vilnius State Univ, Inst Ecol, LT-08412 Vilnius, Lithuania. [Saatchi, Sassan] CALTECH, Jet Prop Lab, Pasadena, CA 94132 USA. RP Bonneaud, C (reprint author), Harvard Univ, Dept Organism & Evolutionary Biol, Museum Comparat Zool, Cambridge, MA 02138 USA. EM cbonneaud@oeb.harvard.edu RI SEHGAL, Ravinder/F-9216-2010; OI SEHGAL, Ravinder/0000-0002-5255-4641; Mila, Borja/0000-0002-6446-0079 FU NSF-NIH Ecology of Infectious Diseases Program [FF-0430146]; Lithuanian State Science and Studies Foundation FX The research was funded by the joint NSF-NIH Ecology of Infectious Diseases Program award FF-0430146 and by the Lithuanian State Science and Studies Foundation. NR 59 TC 27 Z9 28 U1 5 U2 30 PU CAMBRIDGE UNIV PRESS PI NEW YORK PA 32 AVENUE OF THE AMERICAS, NEW YORK, NY 10013-2473 USA SN 0266-4674 J9 J TROP ECOL JI J. Trop. Ecol. PD JUL PY 2009 VL 25 BP 439 EP 447 DI 10.1017/S0266467409006178 PG 9 WC Ecology SC Environmental Sciences & Ecology GA 461CR UT WOS:000267242600009 ER PT J AU Walker, J Ragasa, S Sanders, R Lovell, D McDougal, M AF Walker, James Ragasa, Scott Sanders, Rose Lovell, Don McDougal, Matthew TI Nondestructive Testing Techniques for the Ares I Common Bulkhead Bond Line SO MATERIALS EVALUATION LA English DT Article ID THERMOGRAPHY; SHEAROGRAPHY C1 [Walker, James; McDougal, Matthew] NASA, George C Marshall Space Flight Ctr, Damage Tolerance Assessment Branch EM20, Huntsville, AL 35812 USA. [Ragasa, Scott] Univ Alabama, Huntsville, AL 35899 USA. [Sanders, Rose] Lockheed Martin Space Syst Co, Huntsville Tech Operat, MSFC, Huntsville, AL 35812 USA. RP Walker, J (reprint author), NASA, George C Marshall Space Flight Ctr, Damage Tolerance Assessment Branch EM20, Huntsville, AL 35812 USA. EM james.l.walker@nasa.gov NR 8 TC 0 Z9 0 U1 0 U2 0 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 JUL PY 2009 VL 67 IS 7 BP 774 EP 783 PG 10 WC Materials Science, Characterization & Testing SC Materials Science GA 468XG UT WOS:000267857100002 ER PT J AU Wallace, WT Taylor, LA Liu, Y Cooper, BL Mckay, DS Chen, B Jeevarajan, AS AF Wallace, William T. Taylor, Lawrence A. Liu, Yang Cooper, Bonnie L. McKay, David S. Chen, Bo Jeevarajan, Antony S. TI Lunar dust and lunar simulant activation' and monitoring SO METEORITICS & PLANETARY SCIENCE LA English DT Article ID STANDARD DQ12 QUARTZ; HYDROXYL RADICALS; FLUORESCENCE; TEREPHTHALATE; GENERATION; SURFACE; ULTRASOUND; DOSIMETER; MECHANISM; TOXICITY AB NASA plans to resume human exploration of the Moon in the next decade. One of the pressing concerns is the effect that lunar dust (the fraction of the lunar regolith <20 mu m in diameter) will have oil systems, both human and mechanical, due to the fact that various problems were caused by dust during the Apollo missions. The loss of vacuum integrity in the lunar sample containers during the Apollo era ensured that the present lunar samples are not in the same condition as they were on the Moon; they have been passivated by oxygen and water vapor. To mitigate the harmful effects of lunar dust on humans, methods of "reactivating" the dust must be developed for experimentation, and, ideally, it should be possible to monitor the level of activity to determine methods of deactivating the dust in future lunar habitats. Here we present results demonstrating that simple grinding, as a simple analog to micrometeorite crushing, is capable of substantially activating lunar dust and lunar simulant, and it is possible to determine the level of chemical activity by monitoring the ability of the dust to produce hydroxyl radicals in aqueous Solution. Comparisons between ground samples of lunar dust, lunar simulant, and quartz reveal that ground lunar dust is capable of producing over three times the amount of hydroxyl radicals as lunar simulant and an order of magnitude more than ground quartz. C1 [Wallace, William T.] Univ Space Res Assoc, Houston, TX USA. [Wallace, William T.; Jeevarajan, Antony S.] NASA, Lyndon B Johnson Space Ctr, Habitabil & Environm Factors Div, Houston, TX 77058 USA. [Taylor, Lawrence A.; Liu, Yang] Univ Tennessee, Dept Earth & Planetary Sci, Planetary Geosci Inst, Knoxville, TN 37996 USA. [Cooper, Bonnie L.] Oceaneering Space Syst, Houston, TX 77058 USA. [Chen, Bo] Rice Univ, Smalley Inst Nanoscale Sci & Technol, Houston, TX 77005 USA. RP Wallace, WT (reprint author), Univ Space Res Assoc, Houston, TX USA. EM william.wallace-1@nasa.gov RI Liu, Yang/A-4708-2012 FU NASA Lunar Airborne Dust Toxicity Assessment Group (LADTAG); Planetary Geosciences Institute at the University of Tennessee FX The authors would like to thank Dr. Kelley Bradley and Dr. Dianne Hammond at NASA Lyndon B. Johnson Space Center for their technical assistance with this work and Dr. Ariel Macatangay for his critical review of the manuscript. Additionally, the input and support of the NASA Lunar Airborne Dust Toxicity Assessment Group (LADTAG) has been extremely beneficial. A portion of this study has been funded by a grant to LAT from LADTAG and the Planetary Geosciences Institute at the University of Tennessee. NR 30 TC 16 Z9 18 U1 0 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 JUL PY 2009 VL 44 IS 7 BP 961 EP 970 PG 10 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 502VP UT WOS:000270488700003 ER PT J AU Danielson, LR Righter, K Humayun, M AF Danielson, Lisa R. Righter, Kevin Humayun, Munir TI Trace element chemistry of Cumulus Ridge 04071 pallasite with implications for main group pallasites SO METEORITICS & PLANETARY SCIENCE LA English DT Article ID IRON-METEORITES; CHEMICAL CLASSIFICATION; IIIAB IRONS; METAL; RE; MELT; OLIVINE; GA; FRACTIONATION; EARTH AB Pallasites have long been thought to represent samples from the metallic core-silicate mantle boundary of a small asteroid-sized body, with as many as ten different parent bodies recognized recently. This report focuses on the description, classification, and petrogenetic history of pallasite Cumulus Ridge (CMS) 04071 using electron microscopy and laser ablation ICP-MS. Most olivines are angular in CMS 04071, but there are some minor Occurrences of small rounded olivines, such as in the Eagle Station pallasite. Olivine, chromite, and metal compositions indicate that CMS 04071 can be classified as a Main Group pallasite. The kamacite/taenite partition coefficients (D) for highly siderophile elements (HSE) are all close to 1, but comparison with previous studies on iron meteorites and pallasites shows that variation of some D values is controlled by the Ni content of taenite. D(HSE)(metal/sulfide) for Re, Cu, and Cr all are <1, indicating chalcophile behavior for these three elements, in agreement with experimental D(metal/sulfide) D(HSE)(metal/olivine) are variable, which is perhaps due to small metallic inclusions in the olivine that are present to variable extents in different pallasites. All of these data, together with results from previous Studies, indicate that the CMS pallasites were likely Formed at the core-mantle boundary of a small asteroid, but not necessarily related to the core that produced the IIIAB irons. In addition, they share a similar volatile element depletion to HEDs that is distinct from other bodies such as Earth, Mars, Angrite Parent Body, and the parent body of the brachinites. C1 [Danielson, Lisa R.; Righter, Kevin] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. [Humayun, Munir] Florida State Univ, Dept Geol Sci, Tallahassee, FL 32310 USA. [Humayun, Munir] Florida State Univ, Natl High Magnet Field Lab, Tallahassee, FL 32310 USA. RP Danielson, LR (reprint author), NASA, Lyndon B Johnson Space Ctr, Mailcode JE23,2101 NASA Pkwy, Houston, TX 77058 USA. EM lisa.r.danielson@nasa.gov OI Humayun, Munir/0000-0001-8516-9435 FU NASA [NNG06GF50G] FX We wish to thank Georg Ann Robinson for producing the BSE map of CMS 04071,9. Loan Le provided assistance on the electron microprobe. The MWG and Smithsonian Institution allocated the sample. This research was Supported by a NASA postdoctoral Fellowship to LRD, a NASA RTOP to K. Righter, and NASA grant NNG06GF50G to M. Humayun. The manuscript benefitted from reviews by Henning Haack, Joe Boesenberg, and Alex Ruzicka. We also thank Alex Ruzicka for editorial handling of this manuscript. NR 70 TC 4 Z9 4 U1 1 U2 8 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 1086-9379 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD JUL PY 2009 VL 44 IS 7 BP 1019 EP 1032 PG 14 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 502VP UT WOS:000270488700007 ER PT J AU Abreu, NM Nuth, JAI AF Abreu, N. M. Nuth, J. A. Ill TI IRON SULFIDE FORMATION IN ASTROPHYSICAL ENVIRONMENTS: EXPERIMENTALLY PRODUCED SULFUR-BEARING SILICATE SMOKES SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 72nd Annual Meeting of the Meteoritical-Society CY JUL 13-18, 2009 CL Nancy, FRANCE SP Meteorit Soc, Barringer Crateer Co, Ctr Natl Etudes Spatiales, Ctr Natl Rec Sci, Ctr Rech Petrog & Geochim, Communaute Urbaine Grand Nancy, Conseil Gen Meurthe & Moselle, Inst Natl Sci Univ, Lunar & Planetary Inst, Minist Enseignement Superieur & Rech, Nancy Univ, NASA Cosmochem Program, Planetary Studies Fdn, Reg Lorraine ID DISKS C1 [Abreu, N. M.] Penn State Univ, University Pk, PA 16802 USA. [Nuth, J. A. Ill] Goddard Space Flight Ctr, Astrochem Lab, Greenbelt, MD 20771 USA. EM nma12@psu.edu RI Nuth, Joseph/E-7085-2012 NR 9 TC 0 Z9 0 U1 0 U2 0 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 1086-9379 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD JUL PY 2009 VL 44 SU S BP A16 EP A16 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 461ZO UT WOS:000267314500007 ER PT J AU Bartoschewitz, R Park, J Nagao, K Okazaki, R Kurtz, T AF Bartoschewitz, R. Park, J. Nagao, K. Okazaki, R. Kurtz, Th. TI LUNAR METEORITE SAU 300-NOBLE GAS RECORD SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 72nd Annual Meeting of the Meteoritical-Society CY JUL 13-18, 2009 CL Nancy, FRANCE SP Meteorit Soc, Barringer Crateer Co, Ctr Natl Etudes Spatiales, Ctr Natl rech Sci, Ctr Rech Petrog & Geochim, Communaute Urbaine Grand Nancy, Conseil Gen Meurthe & Moselle, Inst Natl Sci Univ, Lunar & Planetary Inst, Minist Enseignement Superieur & Rech, Nancy Univ, NASA Cosmochem Program, Planetary Studies Fdn, Reg Lorraine ID MINERALOGY; HISTORY C1 [Park, J.] NASA, Lyndon B Johnson Space Ctr, Code KR, ARES, Houston, TX 77058 USA. [Nagao, K.] Univ Tokyo, Grad Sch Sci, Earthquake Chem Lab, Bunkyo Ku, Tokyo 1130033, Japan. [Okazaki, R.] Kyushu Univ, Dept Earth & Planetary Sci, Fac Sci, Fukuoka 8128581, Japan. EM Bartoschewitz.Meteorite-Lab@t-online.de NR 5 TC 1 Z9 1 U1 0 U2 0 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 JUL PY 2009 VL 44 BP A30 EP A30 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 461ZO UT WOS:000267314500035 ER PT J AU Briani, G Gounelle, M Zolensky, ME AF Briani, G. Gounelle, M. Zolensky, M. E. TI (MICRO)XENOLITH SYSTEMATICS IN H CHONDRITES SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 72nd Annual Meeting of the Meteoritical-Society CY JUL 13-18, 2009 CL Nancy, FRANCE SP Meteorit Soc, Barringer Crateer Co, Ctr Natl Etudes Spatiales, Ctr Natl rech Sci, Ctr Rech Petrog & Geochim, Communaute Urbaine Grand Nancy, Conseil Gen Meurthe & Moselle, Inst Natl Sci Univ, Lunar & Planetary Inst, Minist Enseignement Superieur & Rech, Nancy Univ, NASA Cosmochem Program, Planetary Studies Fdn, Reg Lorraine ID FOSSIL MICROMETEORITES; SOLAR-SYSTEM; HOWARDITES; MINERALOGY; PLANETS; ORIGIN C1 [Briani, G.; Gounelle, M.] MNHN, Lab Mineral & Cosmochim Museum, Paris, France. [Briani, G.; Gounelle, M.] CNRS, UMR7202, Paris, France. [Briani, G.] Univ Florence, Dipartimento Astron & Sci Spazio, I-50125 Florence, Italy. [Zolensky, M. E.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. EM briani@mnhn.fr NR 9 TC 0 Z9 0 U1 0 U2 2 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 JUL PY 2009 VL 44 BP A41 EP A41 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 461ZO UT WOS:000267314500057 ER PT J AU Buchanan, PC Zolensky, ME Greenwood, RC Franchi, IA AF Buchanan, P. C. Zolensky, M. E. Greenwood, R. C. Franchi, I. A. TI FOREIGN MATERIALS IN POLYMICT BRECCIAS FROM VESTA SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 72nd Annual Meeting of the Meteoritical-Society CY JUL 13-18, 2009 CL Nancy, FRANCE SP Meteorit Soc, Barringer Crateer Co, Ctr Natl Etudes Spatiales, Ctr Natl rech Sci, Ctr Rech Petrog & Geochim, Communaute Urbaine Grand Nancy, Conseil Gen Meurthe & Moselle, Inst Natl Sci Univ, Lunar & Planetary Inst, Minist Enseignement Superieur & Rech, Nancy Univ, NASA Cosmochem Program, Planetary Studies Fdn, Reg Lorraine ID CARBONACEOUS CHONDRITE CLASTS; HOWARDITES; MINERALOGY C1 [Buchanan, P. C.] Kilgore Coll, Kilgore, TX 75662 USA. [Zolensky, M. E.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. [Greenwood, R. C.; Franchi, I. A.] Open Univ, PSSRI, Milton Keynes MK7 6AA, Bucks, England. EM pbuchanan@kilgore.edu NR 8 TC 2 Z9 2 U1 0 U2 0 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 JUL PY 2009 VL 44 BP A42 EP A42 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 461ZO UT WOS:000267314500060 ER PT J AU Busemann, H Nittler, LR Davidson, J Franchi, IA Messenger, S Nakamura-Messenger, K Palma, RL Pepin, RO AF Busemann, H. Nittler, L. R. Davidson, J. Franchi, I. A. Messenger, S. Nakamura-Messenger, K. Palma, R. L. Pepin, R. O. TI CARBON RAMAN SPECTROSCOPY OF 36 INTERPLANETARY DUST PARTICLES SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 72nd Annual Meeting of the Meteoritical-Society CY JUL 13-18, 2009 CL Nancy, FRANCE SP Meteorit Soc, Barringer Crateer Co, Ctr Natl Etudes Spatiales, Ctr Natl rech Sci, Ctr Rech Petrog & Geochim, Communaute Urbaine Grand Nancy, Conseil Gen Meurthe & Moselle, Inst Natl Sci Univ, Lunar & Planetary Inst, Minist Enseignement Superieur & Rech, Nancy Univ, NASA Cosmochem Program, Planetary Studies Fdn, Reg Lorraine C1 [Busemann, H.] Univ Manchester, SEAES, Manchester M13 9PL, Lancs, England. [Busemann, H.; Nittler, L. R.] Carnegie Inst Washington, DTM, Washington, DC 20005 USA. [Davidson, J.; Franchi, I. A.] Open Univ, PSSRI, Milton Keynes, Bucks, England. [Messenger, S.; Nakamura-Messenger, K.] NASA, JSC Houston, Washington, DC USA. [Palma, R. L.] Minnesota State Univ, Mankato, MN USA. [Palma, R. L.; Pepin, R. O.] Univ Minnesota, Minneapolis, MN USA. EM busemann@manchester.ac.uk RI Davidson, Jemma/B-9453-2013; Davidson, Jemma/K-6828-2013 OI Davidson, Jemma/0000-0002-2788-1130; NR 8 TC 0 Z9 0 U1 0 U2 2 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 JUL PY 2009 VL 44 BP A46 EP A46 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 461ZO UT WOS:000267314500067 ER PT J AU Clemett, SJ Nakamura-Messenger, K Messenger, S Thomas-Keprta, KL Robinson, GA McKay, DS AF Clemett, S. J. Nakamura-Messenger, K. Messenger, S. Thomas-Keprta, K. L. Robinson, G. -A. McKay, D. S. TI MOLECULAR COMPOSITION OF CARBONACEOUS GLOBULES IN THE BELLS (CM2) CHONDRITE SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 72nd Annual Meeting of the Meteoritical-Society CY JUL 13-18, 2009 CL Nancy, FRANCE SP Meteorit Soc, Barringer Crateer Co, Ctr Natl Etudes Spatiales, Ctr Natl rech Sci, Ctr Rech Petrog & Geochim, Communaute Urbaine Grand Nancy, Conseil Gen Meurthe & Moselle, Inst Natl Sci Univ, Lunar & Planetary Inst, Minist Enseignement Superieur & Rech, Nancy Univ, NASA Cosmochem Program, Planetary Studies Fdn, Reg Lorraine ID METEORITE C1 [Clemett, S. J.; Nakamura-Messenger, K.; Thomas-Keprta, K. L.; Robinson, G. -A.] ESCG, Houston, TX 77058 USA. [McKay, D. S.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. EM simon.j.clemett@nasa.gov NR 5 TC 0 Z9 0 U1 2 U2 2 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 JUL PY 2009 VL 44 BP A52 EP A52 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 461ZO UT WOS:000267314500079 ER PT J AU Debaille, V Brandon, AD O'Neill, C Jacobsen, B Yin, QZ AF Debaille, V. Brandon, A. D. O'Neill, C. Jacobsen, B. Yin, Q. -Z. TI TIMESCALE OF MARTIAN MANTLE OVERTURN RECORDED IN NAKHLITE MARTIAN METEORITES SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 72nd Annual Meeting of the Meteoritical-Society CY JUL 13-18, 2009 CL Nancy, FRANCE SP Meteorit Soc, Barringer Crateer Co, Ctr Natl Etudes Spatiales, Ctr Natl rech Sci, Ctr Rech Petrog & Geochim, Communaute Urbaine Grand Nancy, Conseil Gen Meurthe & Moselle, Inst Natl Sci Univ, Lunar & Planetary Inst, Minist Enseignement Superieur & Rech, Nancy Univ, NASA Cosmochem Program, Planetary Studies Fdn, Reg Lorraine ID MAGMA OCEAN; MARS; EARTH C1 [Debaille, V.] Univ Libre Bruxelles, Brussels, Belgium. [Brandon, A. D.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. [O'Neill, C.] Macquarie Univ, N Ryde, NSW 2109, Australia. [Jacobsen, B.; Yin, Q. -Z.] Univ Calif Davis, Davis, CA 95616 USA. EM vdebaill@ulb.ac.be NR 9 TC 0 Z9 0 U1 0 U2 1 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 JUL PY 2009 VL 44 BP A58 EP A58 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 461ZO UT WOS:000267314500092 ER PT J AU Dukes, C Christoffersen, R Keller, L Loeffler, MJ Baragiola, R AF Dukes, C. Christoffersen, R. Keller, L. Loeffler, M. J. Baragiola, R. TI EFFECT OF SPACE RADIATION PROCESSING ON LUNAR SOIL SURFACE CHEMISTRY: X-RAY PHOTOELECTRON SPECTROSCOPY STUDIES SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 72nd Annual Meeting of the Meteoritical-Society CY JUL 13-18, 2009 CL Nancy, FRANCE SP Meteorit Soc, Barringer Crateer Co, Ctr Natl Etudes Spatiales, Ctr Natl rech Sci, Ctr Rech Petrog & Geochim, Communaute Urbaine Grand Nancy, Conseil Gen Meurthe & Moselle, Inst Natl Sci Univ, Lunar & Planetary Inst, Minist Enseignement Superieur & Rech, Nancy Univ, NASA Cosmochem Program, Planetary Studies Fdn, Reg Lorraine C1 [Dukes, C.; Loeffler, M. J.; Baragiola, R.] Univ Virginia, Lab Atom & Surface Phys, Charlottesville, VA 22902 USA. [Christoffersen, R.] Jacobs Technol, ESCG, Mail Code JE23, Houston, TX 77058 USA. [Christoffersen, R.; Keller, L.] NASA, Lyndon B Johnson Space Ctr, ARES, Houston, TX 77058 USA. EM car8r@virginia.edu RI Loeffler, Mark/C-9477-2012 NR 4 TC 0 Z9 0 U1 0 U2 3 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 JUL PY 2009 VL 44 BP A64 EP A64 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 461ZO UT WOS:000267314500104 ER PT J AU Edmunson, J Cohen, BA AF Edmunson, J. Cohen, B. A. TI CHARACTERIZING THE EFFECT OF SHOCK ON ISOTOPIC AGES II: MG-SUITE TROCTOLITE MAJOR ELEMENTS SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 72nd Annual Meeting of the Meteoritical-Society CY JUL 13-18, 2009 CL Nancy, FRANCE SP Meteorit Soc, Barringer Crateer Co, Ctr Natl Etudes Spatiales, Ctr Natl rech Sci, Ctr Rech Petrog & Geochim, Communaute Urbaine Grand Nancy, Conseil Gen Meurthe & Moselle, Inst Natl Sci Univ, Lunar & Planetary Inst, Minist Enseignement Superieur & Rech, Nancy Univ, NASA Cosmochem Program, Planetary Studies Fdn, Reg Lorraine C1 [Edmunson, J.] NASA, George C Marshall Space Flight Ctr, Postdoctoral Program, Washington, DC USA. EM Jennifer.E.Edmunson@nasa.gov NR 10 TC 0 Z9 0 U1 0 U2 0 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 JUL PY 2009 VL 44 BP A66 EP A66 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 461ZO UT WOS:000267314500108 ER PT J AU Flynn, GJ Wirick, S Keller, LP Jacobsen, C Sandford, SA AF Flynn, G. J. Wirick, S. Keller, L. P. Jacobsen, C. Sandford, S. A. TI CARBONATE GRAINS IN ANHYDROUS IDPS SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 72nd Annual Meeting of the Meteoritical-Society CY JUL 13-18, 2009 CL Nancy, FRANCE SP Meteorit Soc, Barringer Crateer Co, Ctr Natl Etudes Spatiales, Ctr Natl Rec Sci, Ctr Rech Petrog & Geochim, Communaute Urbaine Grand Nancy, Conseil Gen Meurthe & Moselle, Inst Natl Sci Univ, Lunar & Planetary Inst, Minist Enseignement Superieur & Rech, Nancy Univ, NASA Cosmochem Program, Planetary Studies Fdn, Reg Lorraine ID DUST; CONDENSATION C1 [Flynn, G. J.] SUNY Coll Plattsburgh, Dept Phys, Plattsburgh, NY 12901 USA. [Wirick, S.; Jacobsen, C.] SUNY Stony Brook, Dept Phys & Astron, Stony Brook, NY 11794 USA. [Keller, L. P.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. [Sandford, S. A.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. EM george.Flynn@plattsburgh.edu RI Jacobsen, Chris/E-2827-2015 OI Jacobsen, Chris/0000-0001-8562-0353 NR 7 TC 0 Z9 0 U1 0 U2 0 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 1086-9379 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD JUL PY 2009 VL 44 SU S BP A71 EP A71 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 461ZO UT WOS:000267314500118 ER PT J AU Flynn, GJ Wirick, S Keller, LP Jacobsen, C Sandford, SA AF Flynn, G. J. Wirick, S. Keller, L. P. Jacobsen, C. Sandford, S. A. TI ORGANIC RIMS ON INDIVIDUAL GRAINS IN CP IDPS: CONSTRAINTS ON THE ORIGIN OF PRE-BIOTIC ORGANIC MATTER SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 72nd Annual Meeting of the Meteoritical-Society CY JUL 13-18, 2009 CL Nancy, FRANCE SP Meteorit Soc, Barringer Crateer Co, Ctr Natl Etudes Spatiales, Ctr Natl Rec Sci, Ctr Rech Petrog & Geochim, Communaute Urbaine Grand Nancy, Conseil Gen Meurthe & Moselle, Inst Natl Sci Univ, Lunar & Planetary Inst, Minist Enseignement Superieur & Rech, Nancy Univ, NASA Cosmochem Program, Planetary Studies Fdn, Reg Lorraine ID INTERPLANETARY DUST C1 [Flynn, G. J.] SUNY Coll Plattsburgh, Dept Phys, Plattsburgh, NY 12901 USA. [Wirick, S.; Jacobsen, C.] SUNY Stony Brook, Dept Phys & Astron, Stony Brook, NY 11794 USA. [Keller, L. P.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. [Sandford, S. A.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. EM george.Flynn@plattsburgh.edu RI Jacobsen, Chris/E-2827-2015 OI Jacobsen, Chris/0000-0001-8562-0353 NR 4 TC 0 Z9 0 U1 0 U2 0 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 1086-9379 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD JUL PY 2009 VL 44 SU S BP A71 EP A71 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 461ZO UT WOS:000267314500117 ER PT J AU Glavin, DP Dworkin, JP AF Glavin, D. P. Dworkin, J. P. TI ENRICHMENT OF L-ISOVALINE BY AQUEOUS ALTERATION ON CI AND CM METEORITE PARENT BODIES SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 72nd Annual Meeting of the Meteoritical-Society CY JUL 13-18, 2009 CL Nancy, FRANCE SP Meteorit Soc, Barringer Crateer Co, Ctr Natl Etudes Spatiales, Ctr Natl rech Sci, Ctr Rech Petrog & Geochim, Communaute Urbaine Grand Nancy, Conseil Gen Meurthe & Moselle, Inst Natl Sci Univ, Lunar & Planetary Inst, Minist Enseignement Superieur & Rech, Nancy Univ, NASA Cosmochem Program, Planetary Studies Fdn, Reg Lorraine ID AMINO-ACIDS C1 [Glavin, D. P.; Dworkin, J. P.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. EM daniel.p.glavin@nasa.gov RI Glavin, Daniel/D-6194-2012; Dworkin, Jason/C-9417-2012 OI Glavin, Daniel/0000-0001-7779-7765; Dworkin, Jason/0000-0002-3961-8997 NR 7 TC 0 Z9 0 U1 0 U2 3 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 JUL PY 2009 VL 44 BP A78 EP A78 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 461ZO UT WOS:000267314500132 ER PT J AU Herrin, JS Zolensky, ME Ito, M Jenniskens, P Shaddad, MH AF Herrin, J. S. Zolensky, M. E. Ito, M. Jenniskens, P. Shaddad, M. H. TI FOSSILIZED SMELTING; REDUCTION TEXTURES IN ALMAHATA SITTA UREILITE SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 72nd Annual Meeting of the Meteoritical-Society CY JUL 13-18, 2009 CL Nancy, FRANCE SP Meteorit Soc, Barringer Crateer Co, Ctr Natl Etudes Spatiales, Ctr Natl rech Sci, Ctr Rech Petrog & Geochim, Communaute Urbaine Grand Nancy, Conseil Gen Meurthe & Moselle, Inst Natl Sci Univ, Lunar & Planetary Inst, Minist Enseignement Superieur & Rech, Nancy Univ, NASA Cosmochem Program, Planetary Studies Fdn, Reg Lorraine ID DISRUPTION C1 [Herrin, J. S.; Zolensky, M. E.; Ito, M.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. [Ito, M.] Lunar & Planetary Inst, Houston, TX 77058 USA. [Jenniskens, P.] SETI Inst, Mountain View, CA USA. [Shaddad, M. H.] Univ Khartoum, Dept Phys, Khartoum, Sudan. EM jason.s.herrin@nasa.gov NR 7 TC 7 Z9 7 U1 0 U2 4 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 JUL PY 2009 VL 44 BP A89 EP A89 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 461ZO UT WOS:000267314500153 ER PT J AU Ito, M Messenger, S AF Ito, M. Messenger, S. TI RARE EARTH ELEMENT MEASUREMENTS OF MELILITE AND FASSAITE IN ALLENDE CAI BY NANOSIMS SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 72nd Annual Meeting of the Meteoritical-Society CY JUL 13-18, 2009 CL Nancy, FRANCE SP Meteorit Soc, Barringer Crateer Co, Ctr Natl Etudes Spatiales, Ctr Natl rech Sci, Ctr Rech Petrog & Geochim, Communaute Urbaine Grand Nancy, Conseil Gen Meurthe & Moselle, Inst Natl Sci Univ, Lunar & Planetary Inst, Minist Enseignement Superieur & Rech, Nancy Univ, NASA Cosmochem Program, Planetary Studies Fdn, Reg Lorraine C1 [Ito, M.] Lunar & Planetary Inst, Houston, TX 77058 USA. [Ito, M.; Messenger, S.] NASA, Lyndon B Johnson Space Ctr, ARES, Houston, TX 77058 USA. EM ito@lpi.usra.edu; scott.r.messenger@nasa.gov NR 4 TC 2 Z9 2 U1 0 U2 3 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 JUL PY 2009 VL 44 BP A97 EP A97 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 461ZO UT WOS:000267314500170 ER PT J AU Kebukawa, Y Nakashima, S Aizawa, K Inoue, T Nakamura-Messenger, K Zolensky, ME AF Kebukawa, Y. Nakashima, S. Aizawa, K. Inoue, T. Nakamura-Messenger, K. Zolensky, M. E. TI SPATIAL DISTRIBUTION OF ORGANIC MATTER IN THE BELLS METEORITE USING NEAR-FIELD INFRARED MICRO-SPECTROSCOPY SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 72nd Annual Meeting of the Meteoritical-Society CY JUL 13-18, 2009 CL Nancy, FRANCE SP Meteorit Soc, Barringer Crateer Co, Ctr Natl Etudes Spatiales, Ctr Natl Rec Sci, Ctr Rech Petrog & Geochim, Communaute Urbaine Grand Nancy, Conseil Gen Meurthe & Moselle, Inst Natl Sci Univ, Lunar & Planetary Inst, Minist Enseignement Superieur & Rech, Nancy Univ, NASA Cosmochem Program, Planetary Studies Fdn, Reg Lorraine C1 [Kebukawa, Y.; Nakashima, S.] Osaka Univ, Dept Earth & Space Sci, Osaka 5600043, Japan. [Aizawa, K.; Inoue, T.] Jasco Co Ltd, Tokyo 1928537, Japan. [Nakamura-Messenger, K.; Zolensky, M. E.] NASA, Lyndon B Johnson Space Ctr, KT, Houston, TX 77058 USA. EM yoko.soleil@ess.sci.osaka-u.ac.jp NR 3 TC 0 Z9 0 U1 0 U2 1 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 1086-9379 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD JUL PY 2009 VL 44 SU S BP A107 EP A107 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 461ZO UT WOS:000267314500190 ER PT J AU Kebukawa, Y Nakashima, S Zolensky, ME AF Kebukawa, Y. Nakashima, S. Zolensky, M. E. TI KINETICS OF ORGANIC MATTER DEGRADATION IN THE MURCHISON METEORITE FOR THE EVALUATION OF CHONDRITE PARENT BODY THERMAL EVOLUTION SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 72nd Annual Meeting of the Meteoritical-Society CY JUL 13-18, 2009 CL Nancy, FRANCE SP Meteorit Soc, Barringer Crateer Co, Ctr Natl Etudes Spatiales, Ctr Natl Rec Sci, Ctr Rech Petrog & Geochim, Communaute Urbaine Grand Nancy, Conseil Gen Meurthe & Moselle, Inst Natl Sci Univ, Lunar & Planetary Inst, Minist Enseignement Superieur & Rech, Nancy Univ, NASA Cosmochem Program, Planetary Studies Fdn, Reg Lorraine ID BODIES C1 [Kebukawa, Y.; Nakashima, S.] Osaka Univ, Dept Earth & Space Sci, Osaka 5600043, Japan. [Zolensky, M. E.] NASA, Lyndon B Johnson Space Ctr, KT, Houston, TX 77058 USA. EM yoko.soleil@ess.sci.osaka-u.ac.jp NR 3 TC 0 Z9 0 U1 0 U2 0 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 1086-9379 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD JUL PY 2009 VL 44 SU S BP A107 EP A107 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 461ZO UT WOS:000267314500189 ER PT J AU Keller, LP Nakamura-Messenger, K Messenger, S AF Keller, L. P. Nakamura-Messenger, K. Messenger, S. TI AMORPHOUS SILICATES IN PRIMITIVE METEORITIC MATERIALS: ACFER 094 AND IDPS SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 72nd Annual Meeting of the Meteoritical-Society CY JUL 13-18, 2009 CL Nancy, FRANCE SP Meteorit Soc, Barringer Crateer Co, Ctr Natl Etudes Spatiales, Ctr Natl rech Sci, Ctr Rech Petrog & Geochim, Communaute Urbaine Grand Nancy, Conseil Gen Meurthe & Moselle, Inst Natl Sci Univ, Lunar & Planetary Inst, Minist Enseignement Superieur & Rech, Nancy Univ, NASA Cosmochem Program, Planetary Studies Fdn, Reg Lorraine ID PRESOLAR; MATRIX C1 [Keller, L. P.; Nakamura-Messenger, K.; Messenger, S.] NASA, Lyndon B Johnson Space Ctr, ARES, Robert M Walker Lab Space Sci, Houston, TX 77058 USA. [Nakamura-Messenger, K.] ESCG Jacobs Technol, Houston, TX 77058 USA. EM Lindsay.P.Keller@nasa.gov NR 6 TC 1 Z9 1 U1 0 U2 6 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 JUL PY 2009 VL 44 BP A108 EP A108 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 461ZO UT WOS:000267314500191 ER PT J AU Malavergne, V Toplis, MJ Berthet, S Jones, J AF Malavergne, V. Toplis, M. J. Berthet, S. Jones, J. TI ARE BENCUBBINITE OR ENSTATITE CHONDRITES THE BUILDING BLOCKS OF MERCURY: IMPLICATIONS FOR INTERNAL STRUCTURE AND THE ORIGIN OF A MAGNETIC FIELD SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 72nd Annual Meeting of the Meteoritical-Society CY JUL 13-18, 2009 CL Nancy, FRANCE SP Meteorit Soc, Barringer Crateer Co, Ctr Natl Etudes Spatiales, Ctr Natl rech Sci, Ctr Rech Petrog & Geochim, Communaute Urbaine Grand Nancy, Conseil Gen Meurthe & Moselle, Inst Natl Sci Univ, Lunar & Planetary Inst, Minist Enseignement Superieur & Rech, Nancy Univ, NASA Cosmochem Program, Planetary Studies Fdn, Reg Lorraine C1 [Malavergne, V.; Berthet, S.] Univ Paris Est, Lab Geomat & Geol Ingenieur G21, EA 4119, F-77454 Champs Sur Marne 2, Marne La Vallee, France. [Toplis, M. J.] Univ Toulouse, CNRS, Lab Dynam Terr & Planetaire, UMR 5562, F-31400 Toulouse, France. [Berthet, S.] Lunar & Planetary Inst, Houston, TX 77058 USA. [Jones, J.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. EM malaverg@univ-mlv.fr NR 0 TC 0 Z9 0 U1 0 U2 3 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 JUL PY 2009 VL 44 BP A132 EP A132 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 461ZO UT WOS:000267314500239 ER PT J AU Meshik, A Hohenberg, C Pravdivtseva, O Frank, D Zolensky, M AF Meshik, A. Hohenberg, C. Pravdivtseva, O. Frank, D. Zolensky, M. TI POSSIBLE PRESENCE OF SPALLATION NEON IN THE OUTER LAYER OF PARTICLE-FREE AEROGEL FLOWN ON BOARD OF THE STARDUST MISSION SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 72nd Annual Meeting of the Meteoritical-Society CY JUL 13-18, 2009 CL Nancy, FRANCE SP Meteorit Soc, Barringer Crateer Co, Ctr Natl Etudes Spatiales, Ctr Natl rech Sci, Ctr Rech Petrog & Geochim, Communaute Urbaine Grand Nancy, Conseil Gen Meurthe & Moselle, Inst Natl Sci Univ, Lunar & Planetary Inst, Minist Enseignement Superieur & Rech, Nancy Univ, NASA Cosmochem Program, Planetary Studies Fdn, Reg Lorraine C1 [Meshik, A.; Hohenberg, C.; Pravdivtseva, O.] Washington Univ, Dept Phys, St Louis, MO 63130 USA. [Frank, D.; Zolensky, M.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. EM am@physics.wustl.edu NR 0 TC 0 Z9 0 U1 0 U2 0 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 JUL PY 2009 VL 44 BP A140 EP A140 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 461ZO UT WOS:000267314500255 ER PT J AU Messenger, S Keller, LP Nakamura-Messenger, K Nguyen, AN AF Messenger, S. Keller, L. P. Nakamura-Messenger, K. Nguyen, A. N. TI STARDUST ABUNDANCE VARIATIONS AMONG INTERPLANETARY DUST PARTICLES SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 72nd Annual Meeting of the Meteoritical-Society CY JUL 13-18, 2009 CL Nancy, FRANCE SP Meteorit Soc, Barringer Crateer Co, Ctr Natl Etudes Spatiales, Ctr Natl rech Sci, Ctr Rech Petrog & Geochim, Communaute Urbaine Grand Nancy, Conseil Gen Meurthe & Moselle, Inst Natl Sci Univ, Lunar & Planetary Inst, Minist Enseignement Superieur & Rech, Nancy Univ, NASA Cosmochem Program, Planetary Studies Fdn, Reg Lorraine ID SILICATE; GRAINS C1 [Messenger, S.; Keller, L. P.; Nakamura-Messenger, K.; Nguyen, A. N.] NASA, Lyndon B Johnson Space Ctr, ARES, Robert M Walker Lab Space Sci, Houston, TX 77058 USA. [Nakamura-Messenger, K.; Nguyen, A. N.] ESCG Jacobs Technol, Houston, TX USA. EM scott.r.messenger@nasa.gov NR 7 TC 0 Z9 0 U1 0 U2 0 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 JUL PY 2009 VL 44 BP A141 EP A141 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 461ZO UT WOS:000267314500257 ER PT J AU Nagao, K Park, J AF Nagao, K. Park, J. TI HETEROGENEOUS NOBLE GAS DISTRIBUTION IN THE NWA 2737 CHASSIGNITE SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 72nd Annual Meeting of the Meteoritical-Society CY JUL 13-18, 2009 CL Nancy, FRANCE SP Meteorit Soc, Barringer Crateer Co, Ctr Natl Etudes Spatiales, Ctr Natl Rec Sci, Ctr Rech Petrog & Geochim, Communaute Urbaine Grand Nancy, Conseil Gen Meurthe & Moselle, Inst Natl Sci Univ, Lunar & Planetary Inst, Minist Enseignement Superieur & Rech, Nancy Univ, NASA Cosmochem Program, Planetary Studies Fdn, Reg Lorraine C1 [Nagao, K.] Univ Tokyo, Earthquake Chem Lab, Grad Sch Sci, Bunkyo Ku, Tokyo 1130033, Japan. [Park, J.] NASA, Lyndon B Johnson Space Ctr, ARES, Houston, TX 77058 USA. NR 4 TC 0 Z9 0 U1 0 U2 0 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 1086-9379 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD JUL PY 2009 VL 44 SU S BP A152 EP A152 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 461ZO UT WOS:000267314500279 ER PT J AU Nakamura, T Noguchi, T Tsuchiyama, A Ushikubo, T Kita, NT Valley, JW Takahata, N Sano, Y Zolensky, ME Kakazu, Y Uesugi, K Nakano, T AF Nakamura, T. Noguchi, T. Tsuchiyama, A. Ushikubo, T. Kita, N. T. Valley, J. W. Takahata, N. Sano, Y. Zolensky, M. E. Kakazu, Y. Uesugi, K. Nakano, T. TI ADDITIONAL EVIDENCE FOR THE PRESENCE OF CHONDRULES IN COMET 81P/WILD 2 SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 72nd Annual Meeting of the Meteoritical-Society CY JUL 13-18, 2009 CL Nancy, FRANCE SP Meteorit Soc, Barringer Crateer Co, Ctr Natl Etudes Spatiales, Ctr Natl rech Sci, Ctr Rech Petrog & Geochim, Communaute Urbaine Grand Nancy, Conseil Gen Meurthe & Moselle, Inst Natl Sci Univ, Lunar & Planetary Inst, Minist Enseignement Superieur & Rech, Nancy Univ, NASA Cosmochem Program, Planetary Studies Fdn, Reg Lorraine ID STARDUST; DUST C1 [Nakamura, T.; Kakazu, Y.] Kyushu Univ, Fukuoka 8128581, Japan. [Noguchi, T.] Ibaraki Univ, Mito, Ibaraki 3108512, Japan. [Tsuchiyama, A.] Osaka Univ, Toyonaka, Osaka 5600043, Japan. [Ushikubo, T.; Kita, N. T.; Valley, J. W.] Univ Wisconsin, Madison, WI 53706 USA. [Takahata, N.; Sano, Y.] Univ Tokyo, Tokyo 1648636, Japan. [Zolensky, M. E.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. [Nakano, T.] Geol Survey Japan, Tsukuba, Ibaraki 3058567, Japan. EM tomoki@geo.kyushu-u.ac.jp RI Valley, John/B-3466-2011 OI Valley, John/0000-0003-3530-2722 NR 6 TC 6 Z9 6 U1 0 U2 0 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 JUL PY 2009 VL 44 BP A153 EP A153 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 461ZO UT WOS:000267314500282 ER PT J AU Nakamura-Messenger, K Messenger, S Keller, LP AF Nakamura-Messenger, K. Messenger, S. Keller, L. P. TI COORDINATED STEM AND NANOSIMS ANALYSIS OF ENSTATITE WHISKERS IN INTERPLANETARY DUST PARTICLES SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 72nd Annual Meeting of the Meteoritical-Society CY JUL 13-18, 2009 CL Nancy, FRANCE SP Meteorit Soc, Barringer Crateer Co, Ctr Natl Etudes Spatiales, Ctr Natl rech Sci, Ctr Rech Petrog & Geochim, Communaute Urbaine Grand Nancy, Conseil Gen Meurthe & Moselle, Inst Natl Sci Univ, Lunar & Planetary Inst, Minist Enseignement Superieur & Rech, Nancy Univ, NASA Cosmochem Program, Planetary Studies Fdn, Reg Lorraine C1 [Nakamura-Messenger, K.; Messenger, S.; Keller, L. P.] NASA, Lyndon B Johnson Space Ctr, Robert M Walker Lab Space Sci, ARES, Houston, TX 77058 USA. ESCG Jacobs Technol, Houston, TX USA. EM keiko.nakamura-1@nasa.gov NR 4 TC 0 Z9 0 U1 0 U2 0 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 JUL PY 2009 VL 44 BP A154 EP A154 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 461ZO UT WOS:000267314500283 ER PT J AU Nguyen, AN Messenger, S AF Nguyen, A. N. Messenger, S. TI IDENTIFICATION OF AN EXTREMELY O-18-RICH PRESOLAR SILICATE GRAIN IN ACFER 094 SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 72nd Annual Meeting of the Meteoritical-Society CY JUL 13-18, 2009 CL Nancy, FRANCE SP Meteorit Soc, Barringer Crateer Co, Ctr Natl Etudes Spatiales, Ctr Natl Rec Sci, Ctr Rech Petrog & Geochim, Communaute Urbaine Grand Nancy, Conseil Gen Meurthe & Moselle, Inst Natl Sci Univ, Lunar & Planetary Inst, Minist Enseignement Superieur & Rech, Nancy Univ, NASA Cosmochem Program, Planetary Studies Fdn, Reg Lorraine ID SOLAR-SYSTEM; STARS; METEORITES; CHONDRITES; SUPERNOVA; STARDUST; SPINEL; DUST C1 [Nguyen, A. N.; Messenger, S.] NASA, JSC, Robert M Walker Lab Space Sci, Washington, DC USA. [Nguyen, A. N.] Jacobs Technol, ESCG, Houston, TX USA. EM lan-anh.n.nguyen@nasa.gov NR 9 TC 0 Z9 0 U1 0 U2 0 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 1086-9379 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD JUL PY 2009 VL 44 SU S BP A157 EP A157 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 461ZO UT WOS:000267314500289 ER PT J AU Nuth, JA AF Nuth, Joseph A., III TI A SIMPLE MECHANISM FOR FRACTIONATING OXYGEN ISOTOPES IN THE SOLAR NEBULA SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 72nd Annual Meeting of the Meteoritical-Society CY JUL 13-18, 2009 CL Nancy, FRANCE SP Meteorit Soc, Barringer Crateer Co, Ctr Natl Etudes Spatiales, Ctr Natl rech Sci, Ctr Rech Petrog & Geochim, Communaute Urbaine Grand Nancy, Conseil Gen Meurthe & Moselle, Inst Natl Sci Univ, Lunar & Planetary Inst, Minist Enseignement Superieur & Rech, Nancy Univ, NASA Cosmochem Program, Planetary Studies Fdn, Reg Lorraine ID HETEROGENEITY; TRANSPORT C1 [Nuth, Joseph A., III] NASA, Goddard Space Flight Ctr, Solar Syst Explorat Div, Greenbelt, MD 20771 USA. EM Joseph.A.Nuth@NASA.gov RI Nuth, Joseph/E-7085-2012 NR 8 TC 0 Z9 0 U1 0 U2 0 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 JUL PY 2009 VL 44 BP A103 EP A103 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 461ZO UT WOS:000267314500182 ER PT J AU Nyquist, LE Shih, CY Reese, YD Irving, AJ AF Nyquist, L. E. Shih, C. -Y. Reese, Y. D. Irving, A. J. TI SM-ND AND RB-SR AGES AND ISOTOPIC SYSTEMATICS FOR NWA 2977, A YOUNG BASALT FROM THE PKT SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 72nd Annual Meeting of the Meteoritical-Society CY JUL 13-18, 2009 CL Nancy, FRANCE SP Meteorit Soc, Barringer Crateer Co, Ctr Natl Etudes Spatiales, Ctr Natl rech Sci, Ctr Rech Petrog & Geochim, Communaute Urbaine Grand Nancy, Conseil Gen Meurthe & Moselle, Inst Natl Sci Univ, Lunar & Planetary Inst, Minist Enseignement Superieur & Rech, Nancy Univ, NASA Cosmochem Program, Planetary Studies Fdn, Reg Lorraine C1 [Nyquist, L. E.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. [Shih, C. -Y.] ESCG Jacobs Sverdrub, Houston, TX 77058 USA. [Reese, Y. D.] Muniz Eng, ESCG, Houston, TX 77058 USA. [Irving, A. J.] Univ Washington, Dept Earth & Space Sci, Seattle, WA 98195 USA. EM laurence.e.nyquist@nasa.gov NR 10 TC 2 Z9 2 U1 0 U2 0 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 JUL PY 2009 VL 44 BP A159 EP A159 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 461ZO UT WOS:000267314500293 ER PT J AU Petitat, M Gounelle, M McKeegan, KD Mostefaoui, S Marrocchi, Y Meibom, A Zolensky, ME AF Petitat, M. Gounelle, M. McKeegan, K. D. Mostefaoui, S. Marrocchi, Y. Meibom, A. Zolensky, M. E. TI (MN)-M-53-(CR)-C-53 SYSTEMATICS OF KAIDUN DOLOMITES SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 72nd Annual Meeting of the Meteoritical-Society CY JUL 13-18, 2009 CL Nancy, FRANCE SP Meteorit Soc, Barringer Crateer Co, Ctr Natl Etudes Spatiales, Ctr Natl Rec Sci, Ctr Rech Petrog & Geochim, Communaute Urbaine Grand Nancy, Conseil Gen Meurthe & Moselle, Inst Natl Sci Univ, Lunar & Planetary Inst, Minist Enseignement Superieur & Rech, Nancy Univ, NASA Cosmochem Program, Planetary Studies Fdn, Reg Lorraine C1 [Petitat, M.; Gounelle, M.; Mostefaoui, S.; Marrocchi, Y.; Meibom, A.] CNRS, LMCM, F-75005 Paris, France. [Petitat, M.; Gounelle, M.; Mostefaoui, S.; Marrocchi, Y.; Meibom, A.] MNHN, UMR 7202, CP52, F-75005 Paris, France. [McKeegan, K. D.] Univ Calif Los Angeles, Dept Earth & Space Sci, Los Angeles, CA 90095 USA. [Zolensky, M. E.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. EM petitat@mnhn.fr NR 7 TC 0 Z9 0 U1 0 U2 0 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 1086-9379 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD JUL PY 2009 VL 44 SU S BP A169 EP A169 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 461ZO UT WOS:000267314500313 ER PT J AU Rankenburg, K Humayun, M Brandon, AD Herrin, JS AF Rankenburg, K. Humayun, M. Brandon, A. D. Herrin, J. S. TI HIGHLY SIDEROPHILE ELEMENTS IN UREILITES SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 72nd Annual Meeting of the Meteoritical-Society CY JUL 13-18, 2009 CL Nancy, FRANCE SP Meteorit Soc, Barringer Crateer Co, Ctr Natl Etudes Spatiales, Ctr Natl rech Sci, Ctr Rech Petrog & Geochim, Communaute Urbaine Grand Nancy, Conseil Gen Meurthe & Moselle, Inst Natl Sci Univ, Lunar & Planetary Inst, Minist Enseignement Superieur & Rech, Nancy Univ, NASA Cosmochem Program, Planetary Studies Fdn, Reg Lorraine C1 [Rankenburg, K.; Humayun, M.] Free Univ Berlin, Inst Geol Wissensch, D-12249 Berlin, Germany. Florida State Univ, Natl High Magnet Field Lab, Tallahassee, FL 32310 USA. Florida State Univ, Dept Geol Sci, Tallahassee, FL 32310 USA. [Brandon, A. D.; Herrin, J. S.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. EM rankenburg@yahoo.de NR 0 TC 0 Z9 0 U1 0 U2 1 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 JUL PY 2009 VL 44 BP A173 EP A173 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 461ZO UT WOS:000267314500321 ER PT J AU Rao, MN Nyquist, LE Sutton, S Huth, J AF Rao, M. N. Nyquist, L. E. Sutton, S. Huth, J. TI SULFUR SPECIATION IN THE MARTIAN REGOLITH COMPONENT IN SHERGOTTITE GLASSES SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 72nd Annual Meeting of the Meteoritical-Society CY JUL 13-18, 2009 CL Nancy, FRANCE SP Meteorit Soc, Barringer Crateer Co, Ctr Natl Etudes Spatiales, Ctr Natl Rec Sci, Ctr Rech Petrog & Geochim, Communaute Urbaine Grand Nancy, Conseil Gen Meurthe & Moselle, Inst Natl Sci Univ, Lunar & Planetary Inst, Minist Enseignement Superieur & Rech, Nancy Univ, NASA Cosmochem Program, Planetary Studies Fdn, Reg Lorraine ID METEORITE C1 [Rao, M. N.] NASA, Lyndon B Johnson Space Ctr, Jocobs ESCG, Houston, TX 77058 USA. [Nyquist, L. E.] NASA, Lyndon B Johnson Space Ctr, ARES, Houston, TX 77058 USA. [Sutton, S.] Univ Chicago, Dept Geol Sci, Chicago, IL 60637 USA. [Huth, J.] Max Planck Inst Chem, D-55128 Mainz, Germany. EM nageswara.rao@nasa.gov NR 9 TC 0 Z9 0 U1 0 U2 0 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1086-9379 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD JUL PY 2009 VL 44 SU S BP A173 EP A173 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 461ZO UT WOS:000267314500322 ER PT J AU Righter, K AF Righter, K. TI CONTROLS ON HIGHLY SIDEROPHILE ELEMENT CONCENTRATIONS IN MARTIAN BASALT: SULFIDE SATURATION AND UNDER-SATURATION SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 72nd Annual Meeting of the Meteoritical-Society CY JUL 13-18, 2009 CL Nancy, FRANCE SP Meteorit Soc, Barringer Crateer Co, Ctr Natl Etudes Spatiales, Ctr Natl rech Sci, Ctr Rech Petrog & Geochim, Communaute Urbaine Grand Nancy, Conseil Gen Meurthe & Moselle, Inst Natl Sci Univ, Lunar & Planetary Inst, Minist Enseignement Superieur & Rech, Nancy Univ, NASA Cosmochem Program, Planetary Studies Fdn, Reg Lorraine ID PLATINUM-GROUP ELEMENTS; SILICATE MELT; LIQUID; GOLD; OLIVINE; RE; IR; PD; RU C1 [Righter, K.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. EM kevin.righter-1@nasa.gov NR 12 TC 0 Z9 0 U1 1 U2 1 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 JUL PY 2009 VL 44 BP A174 EP A174 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 461ZO UT WOS:000267314500324 ER PT J AU Righter, M Lapen, TJ Brandon, AD Beard, BL Shafer, JT AF Righter, M. Lapen, T. J. Brandon, A. D. Beard, B. L. Shafer, J. T. TI LU-HF AND SM-ND ISOTOPE SYSTEMATICS OF ALH84001: EVIDENCE FOR AN ANCIENT ENRICHED MANTLE RESERVOIR ON MARS SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 72nd Annual Meeting of the Meteoritical-Society CY JUL 13-18, 2009 CL Nancy, FRANCE SP Meteorit Soc, Barringer Crateer Co, Ctr Natl Etudes Spatiales, Ctr Natl rech Sci, Ctr Rech Petrog & Geochim, Communaute Urbaine Grand Nancy, Conseil Gen Meurthe & Moselle, Inst Natl Sci Univ, Lunar & Planetary Inst, Minist Enseignement Superieur & Rech, Nancy Univ, NASA Cosmochem Program, Planetary Studies Fdn, Reg Lorraine ID METEORITES C1 [Righter, M.; Lapen, T. J.] Univ Houston, Dept Earth & Atmospher Sci, Houston, TX 77004 USA. [Brandon, A. D.] NASA, Lyndon B Johnson Space Ctr, Washington, DC USA. [Beard, B. L.] Univ Wisconsin, Dept Geol & Geophys, Madison, WI 53706 USA. [Beard, B. L.] NASA, Astrobiol Inst, Washington, DC USA. [Shafer, J. T.] Lunar & Planetary Inst, Houston, TX USA. EM mrighter@uh.edu NR 7 TC 0 Z9 0 U1 1 U2 1 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 JUL PY 2009 VL 44 BP A175 EP A175 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 461ZO UT WOS:000267314500325 ER PT J AU Usui, T McSween, HY Mittlefehldt, DW Prettyman, TH AF Usui, T. McSween, H. Y., Jr. Mittlefehldt, D. W. Prettyman, T. H. TI CHEMICAL MIXING MODEL AND K-TH-TI SYSTEMATICS OF HED METEORITES FOR THE DAWN MISSION SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 72nd Annual Meeting of the Meteoritical-Society CY JUL 13-18, 2009 CL Nancy, FRANCE SP Meteorit Soc, Barringer Crateer Co, Ctr Natl Etudes Spatiales, Ctr Natl rech Sci, Ctr Rech Petrog & Geochim, Communaute Urbaine Grand Nancy, Conseil Gen Meurthe & Moselle, Inst Natl Sci Univ, Lunar & Planetary Inst, Minist Enseignement Superieur & Rech, Nancy Univ, NASA Cosmochem Program, Planetary Studies Fdn, Reg Lorraine ID RAY C1 [Usui, T.; McSween, H. Y., Jr.] Univ Tennessee, Dept Earth & Planetary Sci, Knoxville, TN USA. [Mittlefehldt, D. W.] NASA, Lyndon B Johnson Space Ctr, Washington, DC USA. EM tusui@utk.edu RI Usui, Tomohiro/G-1204-2010 OI Usui, Tomohiro/0000-0002-4653-293X NR 2 TC 0 Z9 0 U1 0 U2 0 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 JUL PY 2009 VL 44 BP A209 EP A209 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 461ZO UT WOS:000267314500394 ER PT J AU Westphal, AJ Anderson, D Butterworth, AL Frank, D Gainsforth, Z Lettieri, R Marchant, W Mendez, B Von Korff, J Zevin, D AF Westphal, A. J. Anderson, D. Butterworth, A. L. Frank, D. Gainsforth, Z. Lettieri, R. Marchant, W. Mendez, B. Von Korff, J. Zevin, D. TI DETECTION EFFICIENCY AND NOISE RATES IN THE STARDUST@HOME INSTRUMENT SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 72nd Annual Meeting of the Meteoritical-Society CY JUL 13-18, 2009 CL Nancy, FRANCE SP Meteorit Soc, Barringer Crateer Co, Ctr Natl Etudes Spatiales, Ctr Natl rech Sci, Ctr Rech Petrog & Geochim, Communaute Urbaine Grand Nancy, Conseil Gen Meurthe & Moselle, Inst Natl Sci Univ, Lunar & Planetary Inst, Minist Enseignement Superieur & Rech, Nancy Univ, NASA Cosmochem Program, Planetary Studies Fdn, Reg Lorraine C1 [Westphal, A. J.; Anderson, D.; Butterworth, A. L.; Gainsforth, Z.; Lettieri, R.; Marchant, W.; Mendez, B.; Von Korff, J.; Zevin, D.] UC Berkeley, Space Sci Lab, Berkeley, CA USA. [Frank, D.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. NR 1 TC 1 Z9 1 U1 0 U2 1 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 JUL PY 2009 VL 44 BP A217 EP A217 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 461ZO UT WOS:000267314500410 ER PT J AU Zolensky, ME Herrin, J Jenniskens, P Friedrich, JM Rumble, D Steele, A Sandford, SA Shaddad, MH Le, L Robinson, GA Morris, RV AF Zolensky, M. E. Herrin, J. Jenniskens, P. Friedrich, J. M. Rumble, D. Steele, A. Sandford, S. A. Shaddad, M. H. Le, L. Robinson, G. A. Morris, R. V. TI MINERALOGY OF THE ALMAHATA SITTA UREILITE SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 72nd Annual Meeting of the Meteoritical-Society CY JUL 13-18, 2009 CL Nancy, FRANCE SP Meteorit Soc, Barringer Crateer Co, Ctr Natl Etudes Spatiales, Ctr Natl rech Sci, Ctr Rech Petrog & Geochim, Communaute Urbaine Grand Nancy, Conseil Gen Meurthe & Moselle, Inst Natl Sci Univ, Lunar & Planetary Inst, Minist Enseignement Superieur & Rech, Nancy Univ, NASA Cosmochem Program, Planetary Studies Fdn, Reg Lorraine C1 [Zolensky, M. E.; Morris, R. V.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. [Herrin, J.; Le, L.; Robinson, G. A.] ESCG Jacobs, Houston, TX 77058 USA. [Jenniskens, P.] SETI Inst, Mountain View, CA 94043 USA. [Friedrich, J. M.] Fordham Univ, Dept Chem, Bronx, NY 10458 USA. [Rumble, D.; Steele, A.] Carnegie Inst Washington, Geophys Lab, Washington, DC 20015 USA. [Sandford, S. A.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Shaddad, M. H.] Univ Khartoum, Dept Phys, Khartoum 11115, Sudan. EM michael.e.zolensky@nasa.gov NR 3 TC 6 Z9 6 U1 0 U2 1 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 JUL PY 2009 VL 44 BP A227 EP A227 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 461ZO UT WOS:000267314500430 ER PT J AU Weislogel, MM Thomas, EA Graf, JC AF Weislogel, M. M. Thomas, E. A. Graf, J. C. TI A Novel Device Addressing Design Challenges for Passive Fluid Phase Separations Aboard Spacecraft SO MICROGRAVITY SCIENCE AND TECHNOLOGY LA English DT Article DE Capillary flow; Microgravity; Partial wetting; Capillary vane structures; Passive phase separations; Two-phase flow; Aqueous systems; Life support systems; Urine Processing ID FLOW; MICROGRAVITY; COALESCENCE AB Capillary solutions have long existed for the control of liquid inventories in spacecraft fluid systems such as liquid propellants, cryogens and thermal fluids for temperature control. Such large length scale, 'low-gravity,' capillary systems exploit container geometry and fluid properties-primarily wetting-to passively locate or transport fluids to desired positions for a variety of purposes. Such methods have only been confidently established if the wetting conditions are known and favorable. In this paper, several of the significant challenges for 'capillary solutions' to low-gravity multiphase fluids management aboard spacecraft are briefly reviewed in light of applications common to life support systems that emphasize the impact of the widely varying wetting properties typical of aqueous systems. A restrictive though no less typifying example of passive phase separation in a urine collection system is highlighted that identifies key design considerations potentially met by predominately capillary solutions. Sample results from novel scale model prototype testing aboard a NASA low-g aircraft are presented that support the various design considerations. C1 [Weislogel, M. M.] Portland State Univ, Portland, OR 97207 USA. [Thomas, E. A.; Graf, J. C.] NASA Johnson Space Ctr, Houston, TX USA. RP Weislogel, MM (reprint author), Portland State Univ, Portland, OR 97207 USA. EM mmw@cecs.pdx.edu; Evan.A.Thomas@nasa.gov; john.c.graf@nasa.gov FU Crew Exploration Vehicle Technical Risk Reduction project FX The authors gratefully acknowledge the contributions of colleagues in the Crew and Thermal Systems Division at NASA Johnson Space Center: J. Sweterlitsch, S. Curley, D. Muirhead, O. Estrada, M. Casteel, M. Callahan, G. Cathey, J. Fraughton and K. Pickering. Funding was generously provided by the Crew Exploration Vehicle Technical Risk Reduction project. NR 30 TC 7 Z9 7 U1 0 U2 16 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0938-0108 J9 MICROGRAVITY SCI TEC JI Microgravity Sci. Technol. PD JUL PY 2009 VL 21 IS 3 BP 257 EP 268 DI 10.1007/s12217-008-9091-7 PG 12 WC Engineering, Aerospace; Thermodynamics; Mechanics SC Engineering; Thermodynamics; Mechanics GA 456GM UT WOS:000266830600005 ER PT J AU Moulton, KD Jamison, JL Baumgarten, TL Speth, A Rothschild, LJ Duboise, SM AF Moulton, K. D. Jamison, J. L. Baumgarten, T. L. Speth, A. Rothschild, L. J. Duboise, S. M. TI Bacteriophage Morphotypes Isolated from a Unique Coastal Mining Site SO MICROSCOPY AND MICROANALYSIS LA English DT Meeting Abstract ID VIRUSES C1 [Moulton, K. D.; Jamison, J. L.; Baumgarten, T. L.; Speth, A.; Duboise, S. M.] Univ So Maine, Dept Appl Sci Med, Portland, ME 04103 USA. [Rothschild, L. J.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Moulton, KD (reprint author), Univ So Maine, Dept Appl Sci Med, 96 Falmouth St,178 Sci Bldg, Portland, ME 04103 USA. FU NASA [EP-07-03, EP-08-02]; NSF [CNS-0521262, DGE-0440560] FX This work was supported by NASA EPSCoR grants EP-07-03 and EP-08-02 and NSF grant CNS-0521262. A. Speth and T. Baumgarten received graduate fellowship support from NSF grant DGE-0440560. The assistance of Naji Akladiss, Maine Department of Environmental Protection, is gratefully acknowledged. NR 5 TC 0 Z9 0 U1 1 U2 3 PU CAMBRIDGE UNIV PRESS PI NEW YORK PA 32 AVENUE OF THE AMERICAS, NEW YORK, NY 10013-2473 USA SN 1431-9276 J9 MICROSC MICROANAL JI Microsc. microanal. PD JUL PY 2009 VL 15 SU 2 BP 956 EP 957 DI 10.1017/S1431927609096494 PG 2 WC Materials Science, Multidisciplinary; Microscopy SC Materials Science; Microscopy GA V20CW UT WOS:000208119100472 ER PT J AU Vander Wal, RL Bryg, VM AF Vander Wal, Randy L. Bryg, Victoria M. TI Jet Soot: Chemical and Structural Characterization via XPS and HRTEM SO MICROSCOPY AND MICROANALYSIS LA English DT Meeting Abstract C1 [Vander Wal, Randy L.] Penn State Univ, Dept Energy & Mineral Engn, EMS Energy Inst, University Pk, PA 16802 USA. [Vander Wal, Randy L.] Penn State Inst Energy & Environm, University Pk, PA 16802 USA. [Bryg, Victoria M.] NASA, USRA, Glenn Res Ctr, Cleveland, OH 44135 USA. RP Vander Wal, RL (reprint author), Penn State Univ, Dept Energy & Mineral Engn, EMS Energy Inst, University Pk, PA 16802 USA. NR 2 TC 0 Z9 0 U1 2 U2 11 PU CAMBRIDGE UNIV PRESS PI NEW YORK PA 32 AVENUE OF THE AMERICAS, NEW YORK, NY 10013-2473 USA SN 1431-9276 J9 MICROSC MICROANAL JI Microsc. microanal. PD JUL PY 2009 VL 15 SU 2 BP 1032 EP 1033 DI 10.1017/S1431927609094951 PG 2 WC Materials Science, Multidisciplinary; Microscopy SC Materials Science; Microscopy GA V20CW UT WOS:000208119100510 ER PT J AU Kovarik, L Yang, F Noebe, RD Mills, MJ AF Kovarik, L. Yang, F. Noebe, R. D. Mills, M. J. TI High Resolution Microscopy Analysis of a New Precipitate Phase in the High-Temperature Shape Memory Alloy Ni30Pt20Ti50 SO MICROSCOPY AND MICROANALYSIS LA English DT Meeting Abstract C1 [Kovarik, L.; Yang, F.; Mills, M. J.] Ohio State Univ, Columbus, OH 43210 USA. [Noebe, R. D.] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. RP Kovarik, L (reprint author), Ohio State Univ, 2041 Coll Rd,Watts Hall 477, Columbus, OH 43210 USA. RI Kovarik, Libor/L-7139-2016 FU NASA FX This project is supported by the NASA Fundamental Aeronautics Program, Supersonics Project and the analytical facilities of the Campus wide Electron Optics Facility at OSU. NR 1 TC 2 Z9 2 U1 0 U2 2 PU CAMBRIDGE UNIV PRESS PI NEW YORK PA 32 AVENUE OF THE AMERICAS, NEW YORK, NY 10013-2473 USA SN 1431-9276 J9 MICROSC MICROANAL JI Microsc. microanal. PD JUL PY 2009 VL 15 SU 2 BP 1402 EP 1403 DI 10.1017/S143192760909730X PG 2 WC Materials Science, Multidisciplinary; Microscopy SC Materials Science; Microscopy GA V20CW UT WOS:000208119100692 ER PT J AU Hou, Z Banday, AJ Gorski, KM AF Hou, Zhen Banday, A. J. Gorski, K. M. TI The hot and cold spots in five-year WMAP data SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE methods: data analysis; cosmic microwave background ID NON-GAUSSIAN STATISTICS; ANISOTROPY-PROBE DATA; SKY MAPS; BACKGROUND-RADIATION; MICROWAVE SKY; PEAKS AB We present an extensive frequentist analysis of the one-point statistics (number, mean, variance, skewness and kurtosis) and two-point correlation functions determined for the local extrema of the cosmic microwave background temperature field observed in five-years of Wilkinson Microwave Anisotropy Probe (WMAP) data. Application of a hypothesis test on the one-point statistics indicates a low variance of hot and cold spots in all frequency bands of the WMAP data. The consistency of the observations with Gaussian simulations of the best-fitting cosmological model is rejected at the 95 per cent confidence level outside the WMAP KQ75 mask and the Northern hemispheres in the Galactic and ecliptic coordinate frames. We demonstrate that it is unlikely that residual Galactic foreground emission contributes to the observed non-Gaussianities. However, the application of a high-pass filter that removes large angular scale power does improve the consistency with the best-fitting cosmological model. Two-point correlation functions of the local extrema are calculated for both the temperature pair product [temperature-temperature (T-T)] and spatial pair-counting [point-point (P-P)]. The T-T observations demonstrate weak correlation on scales below 20 degrees and lie completely below the lower 3 sigma confidence region once various temperature thresholds are applied to the extrema determined for the KQ75 mask and northern sky partitions. The P-P correlation structure corresponds to the clustering properties of the temperature extrema, and provides evidence that it is the large angular-scale structures, and some unusual properties thereof, that are intimately connected to the properties of the hot and cold spots observed in the WMAP five-year data. C1 [Hou, Zhen] Chinese Acad Sci, Purple Mt Observ, Nanjing 210008, Peoples R China. [Hou, Zhen; Banday, A. J.] Max Planck Inst Astrophys, D-85748 Garching, Germany. [Hou, Zhen] Chinese Acad Sci, Grad Univ, Beijing 100049, Peoples R China. [Banday, A. J.] Ctr Etud Spatiale Rayonnements, F-31028 Toulouse 4, France. [Gorski, K. M.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Gorski, K. M.] CALTECH, Pasadena, CA 91125 USA. [Gorski, K. M.] Univ Warsaw Observ, PL-00478 Warsaw, Poland. RP Hou, Z (reprint author), Chinese Acad Sci, Purple Mt Observ, Nanjing 210008, Peoples R China. EM houzhen@mpa-garching.mpg.de FU Max-Planck-Gesellschaft Chinese Academy of Sciences Joint Doctoral Promotion Programme (MPG-CAS-DPP) FX ZH acknowledges the support by Max-Planck-Gesellschaft Chinese Academy of Sciences Joint Doctoral Promotion Programme (MPG-CAS-DPP). We also thank Benjamin D. Wandelt, Hans K. Eriksen and Cheng Li for useful discussions. Some of the results in this paper have been derived using the HEALPIX (Gorski et al. 2005) software and analysis package. We acknowledge use of the Legacy Archive for Microwave Background Data Analysis (LAMBDA). NR 26 TC 8 Z9 8 U1 0 U2 0 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD JUL 1 PY 2009 VL 396 IS 3 BP 1273 EP 1286 DI 10.1111/j.1365-2966.2009.14810.x PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 459AM UT WOS:000267072100006 ER PT J AU Gull, TR Nielsen, E Corcoran, MF Madura, TI Owocki, SP Russell, CMP Hillier, DJ Hamaguchi, K Kober, GV Weis, K Stahl, O Okazaki, AT AF Gull, T. R. Nielsen, E. Corcoran, M. F. Madura, T. I. Owocki, S. P. Russell, C. M. P. Hillier, D. J. Hamaguchi, K. Kober, G. V. Weis, K. Stahl, O. Okazaki, A. T. TI The extended interacting wind structure of Eta Carinae SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE binaries: spectroscopic; stars: individual: Eta Carinae; stars: winds, outflows ID TELESCOPE IMAGING SPECTROGRAPH; X-RAY MINIMUM; EMISSION-LINES; BINARY-SYSTEM; SPECTROSCOPIC EVENT; HOMUNCULUS NEBULA; LIGHT-CURVE; FE II; VARIABILITY; COLLISION AB The highly eccentric binary system, eta Car, provides clues to the transition of massive stars from hydrogen-burning via the CNO cycle to a helium-burning evolutionary state. The fast-moving wind of eta Car B creates a cavity in eta Car A's slower, but more massive, stellar wind, providing an in situ probe. The Hubble Space Telescope/Space Telescope Imaging Spectrograph (HST/STIS), with its high spatial and spectral resolutions, is well matched to follow temporal spatial and velocity variations of multiple wind features. We use observations obtained across 1998-2004 to produce a rudimentary three-dimensional model of the wind interaction in the eta Car system. Broad (+/- 500 km s(-1)) [Fe II] emission line structures extend 0.7 arcsec (similar to 1600 au) from the stellar core. In contrast, [Fe III], [Ar III], [Ne III] and [S III] lines extend only 0.3 arcsec (700 au) from NE to SW and are blue shifted from -500 to +200 km s(-1). All observed spectral features vary with the 5.54-year orbital period. The highly ionized, forbidden emission disappears during the low state, associated with periastron passage. The high-ionization emission originates in the outer wind interaction region that is directly excited by the far-ultraviolet radiation from eta Car B. The HST/STIS spectra reveal a time-varying, distorted paraboloidal structure, caused by the interaction of the massive stellar winds. The model and observations are consistent with the orbital plane aligned with the skirt of the Homunculus. However, the axis of the distorted paraboloid, relative to the major axis of the binary orbit, is shifted in a prograde rotation along the plane, which projected on the sky is from NE to NW. C1 [Gull, T. R.; Nielsen, E.; Kober, G. V.] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA. [Nielsen, E.; Kober, G. V.] Catholic Univ Amer, IACS, Dept Phys, Washington, DC 20064 USA. [Corcoran, M. F.; Hamaguchi, K.] NASA, Goddard Space Flight Ctr, CRESST, Greenbelt, MD 20771 USA. [Corcoran, M. F.; Hamaguchi, K.] NASA, Goddard Space Flight Ctr, Xray Astrophys Lab, Greenbelt, MD 20771 USA. [Corcoran, M. F.] Univ Space Res Assoc, Columbia, MD 20706 USA. [Madura, T. I.; Owocki, S. P.; Russell, C. M. P.] Univ Delaware, Bartol Res Inst, Newark, DE 19716 USA. [Hillier, D. J.] Univ Pittsburgh, Dept Phys & Astron, Pittsburgh, PA 15260 USA. [Hamaguchi, K.] Univ Maryland Baltimore Cty, Dept Phys, Baltimore, MD 21250 USA. [Weis, K.] Ruhr Univ Bochum, Inst Astron, D-44780 Bochum, Germany. [Stahl, O.] Univ Heidelberg, ZAH, Landessternwarte Konigstuhl, D-69117 Heidelberg, Germany. [Okazaki, A. T.] Hokkai Gakuen Univ, Fac Engn, Toyohira Ku, Sapporo, Hokkaido 0628605, Japan. RP Gull, TR (reprint author), NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Code 667, Greenbelt, MD 20771 USA. EM theodore.r.gull@nasa.gov RI Gull, Theodore/D-2753-2012 OI Gull, Theodore/0000-0002-6851-5380 FU NASA Graduate Student Research Programme FX The HST observations were accomplished through STIS GTO, HST GO and HST eta Car Treasury Team programmes. All analysis was done using STIS IDL software tools on data available through the HST eta Car Treasury archive. Don Lindler provided very useful display tools for generating the spectro-images. TIM and CMPR were supported through the NASA Graduate Student Research Programme. NR 49 TC 31 Z9 31 U1 0 U2 0 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 JUL 1 PY 2009 VL 396 IS 3 BP 1308 EP 1328 DI 10.1111/j.1365-2966.2009.14854.x PG 21 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 459AM UT WOS:000267072100009 ER PT J AU Karan, H Knupp, K AF Karan, Haldun Knupp, Kevin TI Radar and Profiler Analysis of Colliding Boundaries: A Case Study SO MONTHLY WEATHER REVIEW LA English DT Article ID ATMOSPHERIC UNDULAR BORES; LAYER CONVERGENCE LINES; SEA-BREEZE FRONT; GRAVITY CURRENT; DOPPLER RADAR; GUST FRONT; THUNDERSTORM OUTFLOW; NUMERICAL-SIMULATION; LABORATORY MODEL; DENSITY-CURRENT AB The kinematics of a head-on collision between two gust fronts, followed by a secondary collision between a third gust front and a bore generated by the initial collision, are described using analyses of Weather Surveillance Radar-1988 Doppler (WSR-88D) and Mobile Integrated Profiling System (MIPS) data. Each gust front involved in the initial collision exhibited a nearly north-south orientation and an east-west movement. The eastward-moving boundary was 2 degrees C colder and moved 7 m s(-1) faster than the westward-moving boundary. Two-dimensional wind retrievals reveal contrasting flows within each gravity current. One exhibited a typical gravity current flow structure, while the other assumed the form of a gravity wave/current hybrid with multiple vortices atop the outflow. One of the after-collision boundaries exhibited multiple radar finelines resembling a solitary wave shortly after the collision. About 1 h after the initial collision, a vigorous gust front intersected the eastward-moving bore several minutes before both circulations were sampled by the MIPS. The MIPS measurements indicate that the gust front displaced the bore upward into a neutral residual layer. The bore apparently propagated upward even farther to the next stable layer between 2 and 3 km AGL. MIPS measurements show that the elevated turbulent bore consisted of an initial vigorous wave, with updraft/downdraft magnitudes of 3 and 26 m s(-1), respectively, followed by several (elevated) waves of decreasing amplitude. C1 [Karan, Haldun; Knupp, Kevin] Univ Alabama, Huntsville, AL 35899 USA. RP Karan, H (reprint author), Stennis Space Ctr, Bldg 1103,Rm 233, Stennis Space Ctr, MS 39529 USA. EM karan@ngi.msstate.edu FU National Science Foundation (NSF) [ATM-0239889, ATM-0533596] FX This research was supported by the National Science Foundation (NSF) under Grants ATM-0239889 and ATM-0533596. The NSF provided support for the BAMEX field study. We acknowledge assistance from NCAR personnel who played an important role in the planning and field campaign phases of BAMEX. NR 38 TC 9 Z9 9 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 JUL PY 2009 VL 137 IS 7 BP 2203 EP 2222 DI 10.1175/2008MWR2763.1 PG 20 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 480YH UT WOS:000268772700009 ER PT J AU Li, L Hong, Y Wang, JH Adler, RF Policelli, FS Habib, S Irwn, D Korme, T Okello, L AF Li, Li Hong, Yang Wang, Jiahu Adler, Robert F. Policelli, Frederick S. Habib, Shahid Irwn, Daniel Korme, Tesfaye Okello, Lawrence TI Evaluation of the real-time TRMM-based multi-satellite precipitation analysis for an operational flood prediction system in Nzoia Basin, Lake Victoria, Africa SO NATURAL HAZARDS LA English DT Article DE Flood prediction; Remote sensing precipitation; TRMM; Capacity building ID XINANJIANG MODEL; CLIMATE-CHANGE; PRODUCTS; CHINA AB Many researchers seek to take advantage of the recently available and virtually uninterrupted supply of satellite-based rainfall information as an alternative and supplement to the ground-based observations in order to implement a cost-effective flood prediction in many under-gauged regions around the world. Recently, NASA Applied Science Program has partnered with USAID and African-RCMRD to implement an operational water-hazard warning system, SERVIR-Africa. The ultimate goal of the project is to build up disaster management capacity in East Africa by providing local governmental officials and international aid organizations a practical decision-support tool in order to better assess emerging flood impacts and to quantify spatial extent of flood risk, as well as to respond to such flood emergencies more expediently. The objective of this article is to evaluate the applicability of integrating NASA's standard satellite precipitation product with a flood prediction model for disaster management in Nzoia, sub-basin of Lake Victoria, Africa. This research first evaluated the TMPA real-time rainfall data against gauged rainfall data from the year 2002 through 2006. Then, the gridded Xinanjiang Model was calibrated to Nzoia basin for period of 1985-2006. Benchmark streamflow simulations were produced with the calibrated hydrological model using the rain gauge and observed streamflow data. Afterward, continuous discharge predictions forced by TMPA 3B42RT real-time data from 2002 through 2006 were simulated, and acceptable results were obtained in comparison with the benchmark performance according to the designated statistic indices such as bias ratio (20%) and NSCE (0.67). Moreover, it is identified that the flood prediction results were improved with systematically bias-corrected TMPA rainfall data with less bias (3.6%) and higher NSCE (0.71). Although the results justify to suggest to us that TMPA real-time data can be acceptably used to drive hydrological models for flood prediction purpose in Nzoia basin, continuous progress in space-borne rainfall estimation technology toward higher accuracy and higher spatial resolution is highly appreciated. Finally, it is also highly recommended that to increase flood forecasting lead time, more reliable and more accurate short- or medium-range quantitative precipitation forecasts is a must. C1 [Li, Li; Hong, Yang; Wang, Jiahu] Univ Oklahoma, Sch Civil Engn & Environm Sci, Ctr Nat Hazard & Disaster Ctr, Natl Weather Ctr, Norman, OK 73019 USA. [Adler, Robert F.; Policelli, Frederick S.; Habib, Shahid] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Adler, Robert F.] Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20740 USA. [Irwn, Daniel] NASA, Marshall Space Flight Ctr, Huntsville, AL 35812 USA. [Korme, Tesfaye; Okello, Lawrence] African Reg Ctr Mapping Resources Dev RCMRD, Nairobi, Kenya. RP Hong, Y (reprint author), Univ Oklahoma, Sch Civil Engn & Environm Sci, Ctr Nat Hazard & Disaster Ctr, Natl Weather Ctr, 202 W Boyd ET,CEC 334, Norman, OK 73019 USA. EM yanghong@ou.edu RI Hong, Yang/D-5132-2009 OI Hong, Yang/0000-0001-8720-242X FU NASA Applied Science Program SERVIR-Africa Project; University of Oklahoma FX The financial support from NASA Applied Science Program SERVIR-Africa Project and from University of Oklahoma is gratefully acknowledged. The authors also thank the RCMRD (Tesfaye Korme and Lawrence Okello) for providing gauged rainfall and streamflow observations over Nzoia Basin. NR 19 TC 55 Z9 59 U1 1 U2 39 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0921-030X EI 1573-0840 J9 NAT HAZARDS JI Nat. Hazards PD JUL PY 2009 VL 50 IS 1 BP 109 EP 123 DI 10.1007/s11069-008-9324-5 PG 15 WC Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences; Water Resources SC Geology; Meteorology & Atmospheric Sciences; Water Resources GA 456GQ UT WOS:000266831100009 ER PT J AU Hong, J Allen, B Grindlay, J Chammas, N Barthelemy, S Baker, R Gehrels, N Nelson, KE Labov, S Collins, J Cook, WR McLean, R Harrison, F AF Hong, J. Allen, B. Grindlay, J. Chammas, N. Barthelemy, S. Baker, R. Gehrels, N. Nelson, K. E. Labov, S. Collins, J. Cook, W. R. McLean, R. Harrison, F. TI Building large area CZT imaging detectors for a wide-field hard X-ray telescope-ProtoEXIST1 SO NUCLEAR INSTRUMENTS & METHODS IN PHYSICS RESEARCH SECTION A-ACCELERATORS SPECTROMETERS DETECTORS AND ASSOCIATED EQUIPMENT LA English DT Article DE X-ray imaging; CZT AB We have constructed a moderately large area (32 cm(2)), fine pixel (2.5 mm pixel, 5 mm thick) CZT imaging detector which constitutes the first section of a detector module (256 cm(2)) developed for a balloon-borne wide-field hard X-ray telescope, ProtoEXIST1. ProtoEXIST1 is a prototype for the High Energy Telescope (HET) in the Energetic X-ray imaging Survey Telescope (EXIST), a next generation space-borne multi-wavelength telescope. We have constructed a large (nearly gapless) detector plane through a modularization scheme by tiling of a large number of 2 cm x 2 cm CZT crystals. Our innovative packaging method is ideal for many applications such as coded-aperture imaging, where a large, continuous detector plane is desirable for the optimal performance. Currently we have been able to achieve an energy resolution of 3.2 keV (FWHM) at 59.6 keV on average, which is exceptional considering the moderate pixel size and the number of detectors in simultaneous operation. We expect to complete two modules (512 cm(2)) within the next few months as more CZT becomes available. We plan to test the performance of these detectors in a near space environment in a series of high altitude balloon flights, the first of which is scheduled for Fall 2009. These detector modules are the first in a series of progressively more sophisticated detector units and packaging schemes planned for ProtoEXIST2 & 3, which will demonstrate the technology required for the advanced CZT imaging detectors (0.6 mm pixel, 4.5 m(2) area) required in EXIST/HET. (C) 2009 Elsevier B.V. All rights reserved. C1 [Hong, J.; Allen, B.; Grindlay, J.; Chammas, N.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Barthelemy, S.; Baker, R.; Gehrels, N.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Nelson, K. E.; Labov, S.; Collins, J.] Lawrence Livermore Natl Lab, Livermore, CA 94550 USA. [Cook, W. R.; McLean, R.; Harrison, F.] CALTECH, Pasadena, CA 91125 USA. RP Hong, J (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM jaesub@head.cfa.harvard.edu RI Gehrels, Neil/D-2971-2012 FU NASA APRA [NNG06WC12G]; US Department of Energy [DE-AC52-07NA27344] FX This work is supported in part by NASA APRA Grant NNG06WC12G. Portions of this work were performed under the auspices of the US Department of Energy by Lawrence Livermore National Laboratory under Contract DE-AC52-07NA27344. NR 9 TC 18 Z9 21 U1 0 U2 3 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 JUL 1 PY 2009 VL 605 IS 3 BP 364 EP 373 DI 10.1016/j.nima.2009.04.004 PG 10 WC Instruments & Instrumentation; Nuclear Science & Technology; Physics, Nuclear; Physics, Particles & Fields SC Instruments & Instrumentation; Nuclear Science & Technology; Physics GA 476HL UT WOS:000268430000020 ER PT J AU Liebe, CC Pollock, R Hannah, B Bartman, R Radulescu, C Rud, M Esposito, JA AF Liebe, Carl Christian Pollock, Randy Hannah, Brett Bartman, Randy Radulescu, Costin Rud, Mike Esposito, Joseph A. TI System for establishing best focus for the Orbiting Carbon Observatory instrument SO OPTICAL ENGINEERING LA English DT Article DE Orbiting Carbon Observatory; spectrometer; focusing; shim ring ID MISSION AB A technology for establishing best focus of an optical system is described. This technology was recently used to establish best focus of the Orbiting Carbon Observatory spectrometers while the instrument was undergoing thermal-vacuum testing. Three piezo-actuated motors were used to adjust the tip, tilt, and piston of a focal plane assembly relative to the spectrometer's optical system. A set of optical displacement sensors measured tip-tilt-piston throughout the focusing process. With best focus established and confirmed using a pupil-slicing technique, the corresponding sensor measurements were used to specify the geometry and dimensions of a precision-ground shim ring. (C) 2009 Society of Photo-Optical Instrumentation Engineers. [DOI:10.1117/1.3180867] C1 [Liebe, Carl Christian; Hannah, Brett; Bartman, Randy; Radulescu, Costin; Rud, Mike] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Pollock, Randy; Esposito, Joseph A.] Hamilton Sundstrand Corp, Pomona, CA 91767 USA. RP Liebe, CC (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM Carl.c.liebe@jpl.nasa.gov NR 9 TC 4 Z9 4 U1 1 U2 2 PU SPIE-SOC PHOTOPTICAL INSTRUMENTATION ENGINEERS PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98225 USA SN 0091-3286 J9 OPT ENG JI Opt. Eng. PD JUL PY 2009 VL 48 IS 7 AR 073605 DI 10.1117/1.3180867 PG 9 WC Optics SC Optics GA 477AX UT WOS:000268489400009 ER PT J AU Parker, DM Balazs, GH King, CS Katahira, L Gilmartin, W AF Parker, Denise M. Balazs, George H. King, Cheryl S. Katahira, Larry Gilmartin, William TI Short-Range Movements of Hawksbill Turtles (Eretmochelys imbricata) from Nesting to Foraging Areas within the Hawaiian Islands SO PACIFIC SCIENCE LA English DT Article ID MIGRATIONS AB Hawksbill sea turtles, Eretmochelys imbricata, reside around the main Hawaiian Islands but are not common. Flipper-tag recoveries and satellite tracking of hawksbills worldwide have shown variable distances in post-nesting travel, with migrations between nesting beaches and foraging areas ranging from 35 to 2,425 kin. Nine hawksbill turtles were tracked within the Hawaiian Islands using satellite telemetry. Turtles traveled distances ranging from 90 to 345 km and took between 5 to 18 days to complete the transit front nesting to foraging areas. Results of this study suggest that movements of Hawaiian hawksbills are relatively short-ranged, and surveys of their foraging areas should be conducted to assess status of the habitat to enhance conservation and management of these areas. C1 [Parker, Denise M.; Balazs, George H.] NOAA, Natl Marine Fisheries Serv, Pacific Isl Fisheries Sci Ctr, Honolulu, HI 96822 USA. [Parker, Denise M.] Univ Hawaii, Joint Inst Marine & Atmospher Res, Honolulu, HI 96822 USA. [King, Cheryl S.; Gilmartin, William] Hawaii Wildlife Fund, Maui, HI 96779 USA. [Katahira, Larry] Hawaii Volcanoes Natl Pk, Hawaii Natl Pk, HI 96718 USA. RP Parker, DM (reprint author), NOAA, Natl Marine Fisheries Serv, Pacific Isl Fisheries Sci Ctr, 2570 Dole St, Honolulu, HI 96822 USA. EM Denise.Parker@noaa.gov NR 50 TC 10 Z9 17 U1 1 U2 11 PU UNIV HAWAII PRESS PI HONOLULU PA 2840 KOLOWALU ST, HONOLULU, HI 96822 USA SN 0030-8870 J9 PAC SCI JI Pac. Sci. PD JUL PY 2009 VL 63 IS 3 BP 371 EP 382 DI 10.2984/049.063.0306 PG 12 WC Marine & Freshwater Biology; Zoology SC Marine & Freshwater Biology; Zoology GA 462KJ UT WOS:000267351000006 ER PT J AU Batra, AK Alim, MA Currie, JR Aggarwal, MD AF Batra, A. K. Alim, Mohammad A. Currie, James R. Aggarwal, M. D. TI The electrical response of the modified lead titanate-based thick films SO PHYSICA B-CONDENSED MATTER LA English DT Article DE Pyroelectric; Infrared sensor; Lead titanate; Thick films ID PYROELECTRIC PROPERTIES; CERAMICS; DETECTOR; SENSORS; CASNO3 AB The modified lead titanate (PT) based thick films were fabricated using thick film transfer (TFT) technique. The pyroelectric and dielectric behavior ascertained plausible usage as infrared detectors for these films. The conduction processes in these films are represented by the development of an equivalent circuit model that portrays a near perfect dielectric material containing traps. Various "materials' figures-of-merit" of modified PT films are determined for their potential use as infrared detector. Based on existing information these material properties are found to be reasonable. (C) 2009 Elsevier B.V. All rights reserved. C1 [Alim, Mohammad A.] Alabama A&M Univ, Dept Elect Engn, Huntsville, AL 35762 USA. [Batra, A. K.; Aggarwal, M. D.] Alabama A&M Univ, Dept Phys, Huntsville, AL 35762 USA. [Currie, James R.] NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA. RP Alim, MA (reprint author), Alabama A&M Univ, Dept Elect Engn, POB 297, Huntsville, AL 35762 USA. EM ashok.batra@aamu.edu; mohammad.alim@aamu.edu NR 26 TC 7 Z9 7 U1 1 U2 1 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0921-4526 EI 1873-2135 J9 PHYSICA B JI Physica B PD JUL 1 PY 2009 VL 404 IS 14-15 BP 1905 EP 1911 DI 10.1016/j.physb.2009.02.024 PG 7 WC Physics, Condensed Matter SC Physics GA 463DB UT WOS:000267408000007 ER PT J AU Smith, DD Myneni, K Odutola, JA Diels, JC AF Smith, David D. Myneni, Krishna Odutola, Jamiu A. Diels, J. C. TI Enhanced sensitivity of a passive optical cavity by an intracavity dispersive medium SO PHYSICAL REVIEW A LA English DT Article ID ELECTROMAGNETICALLY INDUCED TRANSPARENCY; LIGHT; LASER; MODE; PROPAGATION; RESONATORS AB The pushing of the modes of a Fabry-Perot cavity by an intracavity rubidium cell is measured. The scale factor of the modes is increased by the anomalous dispersion and is inversely proportional to the sum of the effective group index and an additional cavity delay factor that arises from the variation of the Rb absorption over a free spectral range. This additional positive feedback further increases the effect of the anomalous dispersion and goes to zero at the lasing threshold. The mode width does not grow as fast as the scale factor as the intracavity absorption is increased resulting in enhanced measurement sensitivities. For absorptions larger than the scale factor pole, the atom-cavity response is multivalued and mode splitting occurs. C1 [Smith, David D.] NASA, George C Marshall Space Flight Ctr, Spacecraft & Vehicle Syst Dept, Huntsville, AL 35812 USA. [Smith, David D.; Myneni, Krishna] Univ Alabama, Dept Phys, Huntsville, AL 35899 USA. [Myneni, Krishna] USA, RDECOM, AMSRD AMR WS ST, Redstone Arsenal, AL 35899 USA. [Odutola, Jamiu A.] Alabama A&M Univ, Dept Nat & Phys Sci Chem, Normal, AL 35762 USA. [Diels, J. C.] Univ New Mexico, Dept Phys & Astron, Albuquerque, NM 87131 USA. RP Smith, DD (reprint author), NASA, George C Marshall Space Flight Ctr, Spacecraft & Vehicle Syst Dept, EV43, Huntsville, AL 35812 USA. NR 31 TC 25 Z9 25 U1 1 U2 8 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 JUL PY 2009 VL 80 IS 1 AR 011809 DI 10.1103/PhysRevA.80.011809 PG 4 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA 478VP UT WOS:000268616900027 ER PT J AU Rahman, R Park, SH Cole, JH Greentree, AD Muller, RP Klimeck, G Hollenberg, LCL AF Rahman, Rajib Park, Seung H. Cole, Jared H. Greentree, Andrew D. Muller, Richard P. Klimeck, Gerhard Hollenberg, Lloyd C. L. TI Atomistic simulations of adiabatic coherent electron transport in triple donor systems SO PHYSICAL REVIEW B LA English DT Article ID NEMO 3-D; QUANTUM DOTS; WAVE-GUIDES; ATOM; SEMICONDUCTORS; PASSAGE AB A solid-state analog of stimulated Raman adiabatic passage can be implemented in a triple-well solid-state system to coherently transport an electron across the wells with exponentially suppressed occupation in the central well at any point of time. Termed coherent-tunneling adiabatic passage (CTAP), this method provides a robust way to transfer quantum information encoded in the electronic spin across a chain of quantum dots or donors. Using large-scale atomistic tight-binding simulations involving over 3.5 x 10(6) atoms, we verify the existence of a CTAP pathway in a realistic solid-state system: gated triple donors in silicon. Realistic gate profiles from commercial tools were combined with tight-binding methods to simulate gate control of the donor to donor tunnel barriers in the presence of crosstalk. As CTAP is an adiabatic protocol, it can be analyzed by solving the time-independent problem at various stages of the pulse justifying the use of time-independent tight-binding methods to this problem. This work also involves the first atomistic treatment to translate the three-state-based quantum-optics type of modeling into a solid-state description beyond the ideal localization assumption. Our results show that a three-donor CTAP transfer, with interdonor spacing of 15 nm can occur on time scales greater than 23 ps, well within experimentally accessible regimes. The method not only provides a tool to guide future CTAP experiments but also illuminates the possibility of system engineering to enhance control and transfer times. C1 [Rahman, Rajib; Park, Seung H.; Klimeck, Gerhard] Purdue Univ, Network Computat Nanotechnol, W Lafayette, IN 47907 USA. [Cole, Jared H.] Univ Karlsruhe, DFG, CFN, D-76128 Karlsruhe, Germany. [Cole, Jared H.] Univ Karlsruhe, Inst Theoret Festkorperphys, D-76128 Karlsruhe, Germany. [Cole, Jared H.; Greentree, Andrew D.; Hollenberg, Lloyd C. L.] Univ Melbourne, Sch Phys, Ctr Quantum Comp Technol, Melbourne, Vic 3010, Australia. [Muller, Richard P.] Sandia Natl Labs, Albuquerque, NM 87185 USA. [Klimeck, Gerhard] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Rahman, R (reprint author), Purdue Univ, Network Computat Nanotechnol, W Lafayette, IN 47907 USA. EM rrahman@purdue.edu; lloydch@unimelb.edu.au RI Cole, Jared/G-2992-2010; Hollenberg, Lloyd/B-2296-2010; Greentree, Andrew/A-8503-2008; Klimeck, Gerhard/A-1414-2012; OI Cole, Jared/0000-0002-8943-6518; Greentree, Andrew/0000-0002-3505-9163; Klimeck, Gerhard/0000-0001-7128-773X; Rahman, Rajib/0000-0003-1649-823X NR 40 TC 20 Z9 20 U1 0 U2 9 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 JUL PY 2009 VL 80 IS 3 AR 035302 DI 10.1103/PhysRevB.80.035302 PG 7 WC Physics, Condensed Matter SC Physics GA 478VX UT WOS:000268617800074 ER PT J AU Shebalin, JV AF Shebalin, John V. TI Plasma relaxation and the turbulent dynamo SO PHYSICS OF PLASMAS LA English DT Article DE Fourier series; plasma magnetohydrodynamics; plasma simulation; plasma turbulence ID FREE MAGNETIC FIELDS; MAGNETOHYDRODYNAMIC TURBULENCE; HYDROMAGNETIC TURBULENCE; ISOTROPIC TURBULENCE; HOMOGENEOUS TURBULENCE; ABSOLUTE EQUILIBRIUM; NUMERICAL-SIMULATION; BROKEN ERGODICITY; FLUCTUATIONS; GENERATION AB Ideal magnetohydrodynamic (MHD) turbulence may be represented by finite Fourier series whose independent coefficients form a canonical ensemble described by a Gaussian probability density function containing a Hermitian covariance matrix with positive eigenvalues. When the eigenvalues at lowest wave number are very small, a large-scale coherent structure appears: a turbulent dynamo, which is seen in computations. A theoretical explanation is given and contains Taylor's theory of force-free states. Numerical effects are examined and it is shown that larger grid sizes and smaller time steps provide for better resolution of coherent structure. Ideal hydrodynamic (HD) turbulence is examined and the results are compared and contrasted with those of ideal MHD turbulence. In particular, coherent structure appears in ideal MHD turbulence at the lowest wave number, but can occur in ideal HD turbulence only at the highest wave numbers in a simulation. In the case of real, i.e., dissipative flows, coherent structure and broken ergodicity are expected to occur in MHD turbulence at the largest scale. However, real HD turbulence at all scales and real MHD turbulence at all scales but the largest are expected to be ergodic. C1 NASA, Lyndon B Johnson Space Ctr, Astromat Res & Explorat Sci Off, Houston, TX 77058 USA. RP Shebalin, JV (reprint author), NASA, Lyndon B Johnson Space Ctr, Astromat Res & Explorat Sci Off, Houston, TX 77058 USA. NR 75 TC 10 Z9 10 U1 0 U2 2 PU AMER INST PHYSICS PI MELVILLE PA 1305 WALT WHITMAN RD, STE 300, MELVILLE, NY 11747-4501 USA SN 1070-664X EI 1089-7674 J9 PHYS PLASMAS JI Phys. Plasmas PD JUL PY 2009 VL 16 IS 7 AR 072301 DI 10.1063/1.3159866 PG 14 WC Physics, Fluids & Plasmas SC Physics GA 478UZ UT WOS:000268615200020 ER PT J AU Williams, DA Greeley, R Fergason, RL Kuzmin, R McCord, TB Combe, JP Head, JW Xiao, L Manfredi, L Poulet, F Pinet, P Baratoux, D Plaut, JJ Raitala, J Neukum, G AF Williams, David A. Greeley, Ronald Fergason, Robin L. Kuzmin, Ruslan McCord, Thomas B. Combe, Jean-Phillipe Head, James W., III Xiao, Long Manfredi, Leon Poulet, Francois Pinet, Patrick Baratoux, David Plaut, Jeffrey J. Raitala, Jouko Neukum, Gerhard CA HRSC Co-Investigator Team TI The Circum-Hellas Volcanic Province, Mars: Overview SO PLANETARY AND SPACE SCIENCE LA English DT Article; Proceedings Paper CT European Mars Science and Exploration Conference CY NOV 12-16, 2007 CL ESA European Space Res & Technol Ctr, Noordwijk, NETHERLANDS HO ESA European Space Res & Technol Ctr DE Mars volcanism; Mars express; Remote sensing; Crater statistics ID LASER ALTIMETER; TYRRHENA PATERA; GLOBAL SURVEYOR; CRATERING RATE; SURFACE; EVOLUTION; GEOLOGY; ICE; EXPRESS; REGION AB Building on previous studies of volcanoes around the Hellas basin with new studies of imaging (High-Resolution Stereo Camera (HRSC), Thermal Emission Imaging System (THEMIS), Mars Orbiter Camera (MOC), High-Resolution Imaging Science Experiment (HiRISE), Context Imager (CTX)), multispectral (HRSC, Observatoire pour la Mineralogie, l'Eau, les Glaces et l'Activite (OMEGA)), topographic (Mars Orbiter Laser Altimeter (MOLA)) and gravity data, we define a new Martian volcanic province as the Circum-Hellas Volcanic Province (CHVP). With an area of >2.1 million km(2), it contains the six oldest central vent volcanoes on Mars, which formed after the Hellas impact basin, between 4.0 and 3.6 Ga. These volcanoes mark a transition from the flood volcanism that formed Malea Planum similar to 3.8 Ga. to localized edifice-building eruptions. The CHVP volcanoes have two general morphologies: (1) shield-like edifices (Tyrrhena, Hadriaca, and Amphitrites Paterae), and (2) caldera-like depressions surrounded by ridged plains (Peneus, Malea, and Pityusa Paterae). Positive gravity anomalies are found at Tyrrhena, Hadriaca, and Amphitrites, perhaps indicative of dense magma bodies below the surface. The lack of positive-relief edifices and weak gravity anomalies at Peneus, Malea, and Pityusa suggest a fundamental difference in their formation, styles of eruption, and/or compositions. The northernmost volcanoes, the similar to 3.7-3.9 Ga Tyrrhena and Hadriaca Paterae, have low slopes, well-channeled flanks, and smooth caldera floors (at tens of meters/pixel scale), indicative of volcanoes formed from poorly consolidated pyroclastic deposits that have been modified by fluvial and aeolian erosion and deposition. The similar to 3.6 Ga Amphitrites Patera also has a well-channeled flank, but it and the similar to 3.8 Ga Peneus Patera are dominated by scalloped and pitted terrain, pedestal and ejecta flow craters, and a general 'softened' appearance. This morphology is indicative not only of surface materials subjected to periglacial processes involving water ice, but also of a surface composed of easily eroded materials such as ash and dust. The southernmost volcanoes, the similar to 3.8 Ga Malea and Pityusa Paterae, have no channeled flanks, no scalloped and pitted terrain, and lack the 'softened' appearance of their surfaces, but they do contain pedestal and ejecta flow craters and large, smooth, bright plateaus in their central depressions. This morphology is indicative of a surface with not only a high water ice content, but also a more consolidated material that is less susceptible to degradation (relative to the other four volcanoes). We suggest that Malea and Pityusa (and possibly Peneus) Paterae are Martian equivalents to Earth's giant calderas (e.g., Yellowstone, Long Valley) that erupted large volumes of volcanic materials, and that Malea and Pityusa are probably composed of either lava flows or ignimbrites. HRSC and OMEGA spectral data indicate that dark gray to slightly red materials (often represented as blue or black pixels in HRSC color images), found in the patera floors and topographic lows throughout the CHVP, have a basaltic composition. A key issue is whether this dark material represents concentrations of underlying basaltic material eroded by various processes and exposed by aeolian winnowing, or if the material was transported from elsewhere on Mars by regional winds. Understanding the provenance of these dark materials may be the key to understanding the volcanic diversity of the Circum-Hellas Volcanic Province. (C) 2008 Elsevier Ltd. All rights reserved. C1 [Williams, David A.; Greeley, Ronald; Fergason, Robin L.; Xiao, Long; Manfredi, Leon] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85287 USA. [Kuzmin, Ruslan] Russian Acad Sci, Vernadsky Inst, Moscow 117975, Russia. [McCord, Thomas B.; Combe, Jean-Phillipe] Bear Fight Ctr, Winthrop, WA 98862 USA. [Head, James W., III] Brown Univ, Dept Geol Sci, Providence, RI 02912 USA. [Xiao, Long] China Univ Geosci, Fac Earth Sci, Wuhan 430074, Peoples R China. [Poulet, Francois] Univ Paris 11, Inst Astrophys Spatiale, F-91405 Orsay, France. [Pinet, Patrick; Baratoux, David] Univ Toulouse 3, CNRS, Observ Midi Pyrenees, Lab Dynam Terrestre & Planetaire,UMR 5562, F-31400 Toulouse, France. [Plaut, Jeffrey J.] NASA, Prop Lab, Pasadena, CA 91109 USA. [Raitala, Jouko] Univ Oulu, Astron Div, Dept Phys Sci, Oulu, Finland. [Neukum, Gerhard] Free Univ Berlin, Dept Earth Sci, Inst Geosci Planetary Sci & Remote Sensing, D-12249 Berlin, Germany. RP Williams, DA (reprint author), Arizona State Univ, Sch Earth & Space Explorat, Box 871404, Tempe, AZ 85287 USA. EM David.Williams@asu.edu; greeley@asu.edu; rfergason@usgs.gov; rok@geokhi.ru; mccordtb@aol.com; jean-philippe_combe@bearfightcenter.com; James_Head@brown.edu; longxiao@cug.edu.cn; lmanfred@asu.edu; francois.poulet@ias.u-psud.fr; barataoux@dtp.obs-mip.fr; pinet@dtp.obs-mip.fr; plaut@mail.jpl.nasa.gov; jraitala@sun3.oulu.fi; gneukum@zedat.fu-berlin.de RI Baratoux, David/H-6006-2012 OI Baratoux, David/0000-0002-1785-5262 NR 111 TC 42 Z9 42 U1 0 U2 20 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 JUL PY 2009 VL 57 IS 8-9 SI SI BP 895 EP 916 DI 10.1016/j.pss.2008.08.010 PG 22 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 477QM UT WOS:000268533600002 ER PT J AU Dehant, V Folkner, W Renotte, E Orban, D Asmar, S Balmino, G Barriot, JP Benoist, J Biancale, R Biele, J Budnik, F Burger, S de Viron, O Hausler, B Karatekin, O Le Maistre, S Lognonne, P Menvielle, M Mitrovic, M Patzold, M Rivoldini, A Rosenblatt, P Schubert, G Spohn, T Tortora, P Van Hoolst, T Witasse, O Yseboodt, M AF Dehant, Veronique Folkner, William Renotte, Etienne Orban, Daniel Asmar, Sami Balmino, Georges Barriot, Jean-Pierre Benoist, Jeremy Biancale, Richard Biele, Jens Budnik, Frank Burger, Stefaan de Viron, Olivier Haeusler, Bernd Karatekin, Ozgur Le Maistre, Sebastien Lognonne, Philippe Menvielle, Michel Mitrovic, Michel Paetzold, Martin Rivoldini, Attilio Rosenblatt, Pascal Schubert, Gerald Spohn, Tilman Tortora, Paolo Van Hoolst, Tim Witasse, Olivier Yseboodt, Marie TI Lander radioscience for obtaining the rotation and orientation of Mars SO PLANETARY AND SPACE SCIENCE LA English DT Article; Proceedings Paper CT European Mars Science and Exploration Conference CY NOV 12-16, 2007 CL ESA European Space Res & Technol Ctr, Noordwijk, NETHERLANDS HO ESA European Space Res & Technol Ctr DE Radioscience; X-band signal; Mars nutation; Mars length-of-day ID SEASONAL MASS REDISTRIBUTION; FREE CORE NUTATION; INTERIOR STRUCTURE; CHANDLER-WOBBLE; MARTIAN MANTLE; INSOLATION QUANTITIES; GLOBAL SURVEYOR; MAGNETIC-FIELD; GRAVITY-FIELD; EVOLUTION AB The paper presents the concept, the objectives, the approach used, and the expected performances and accuracies of a radioscience experiment based on a radio link between the Earth and the surface of Mars. This experiment involves radioscience equipment installed on a lander at the surface of Mars. The experiment with the generic name lander radioscience (LaRa) consists of an X-band transponder that has been designed to obtain, over at least one Martian year, two-way Doppler measurements from the radio link between the ExoMars lander and the Earth (ExoMars is an ESA mission to Mars due to launch in 2013). These Doppler measurements will be used to obtain Mars' orientation in space and rotation (precession and nutations, and length-of-day variations). More specifically, the relative position of the lander on the surface of Mars with respect to the Earth ground stations allows reconstructing Mars' time varying orientation and rotation in space. Precession will be determined with an accuracy better by a factor of 4 (better than the 0.1% level) with respect to the present-day accuracy after only a few months at the Martian surface. This precession determination will, in turn, improve the determination of the moment of inertia of the whole planet (mantle plus core) and the radius of the core: for a specific interior composition or even for a range of possible compositions, the core radius is expected to be determined with a precision decreasing to a few tens of kilometers. A fairly precise measurement of variations in the orientation of Mars' spin axis will enable, in addition to the determination of the moment of inertia of the core, an even better determination of the size of the core via the core resonance in the nutation amplitudes. When the core is liquid, the free core nutation (FCN) resonance induces a change in the nutation amplitudes, with respect to their values for a solid planet, at the percent level in the large semi-annual prograde nutation amplitude and even more (a few percent, a few tens of percent or more, depending on the FCN period) for the retrograde terannual nutation amplitude. The resonance amplification depends on the size, moment of inertia, and flattening of the core. For a large core, the amplification can be very large, ensuring the detection of the FCN, and determination of the core moment of inertia. The measurement of variations in Mars' rotation also determines variations of the angular momentum due to seasonal mass transfer between the atmosphere and ice caps. Observations even for a short period of 180 days at the surface of Mars will decrease the uncertainty by a factor of two with respect to the present knowledge of these quantities (at the 10% level). The ultimate objectives of the proposed experiment are to obtain information on Mars' interior and on the sublimation/condensation Of CO2 in Mars' atmosphere. Improved knowledge of the interior will help us to better understand the formation and evolution of Mars. Improved knowledge of the CO2 sublimation/condensation cycle will enable better understanding of the circulation and dynamics of Mars' atmosphere. (C) 2008 Elsevier Ltd. All rights reserved. C1 [Dehant, Veronique; Karatekin, Ozgur; Le Maistre, Sebastien; Mitrovic, Michel; Rivoldini, Attilio; Rosenblatt, Pascal; Van Hoolst, Tim; Yseboodt, Marie] ROB, B-1180 Brussels, Belgium. [Folkner, William; Asmar, Sami] Jet Prop Lab, Pasadena, CA USA. [Orban, Daniel; Burger, Stefaan] OMP, Louvain, Belgium. [Barriot, Jean-Pierre] Univ Polynesie Francaise, Faaa, Fr Polynesia. [Biele, Jens; Spohn, Tilman] DLR, Deutsch Zentrum Luft & Raumfahrt, Berlin, Germany. [de Viron, Olivier; Lognonne, Philippe] Univ Paris 07, Paris, France. [de Viron, Olivier; Lognonne, Philippe] IPGP, Paris, France. [Haeusler, Bernd] Univ Bundeswehr, Munich, Germany. [Menvielle, Michel] Ctr Etud Environm Terrestre & Planetaire CETP, Paris, France. [Paetzold, Martin] Univ Cologne, D-5000 Cologne 41, Germany. [Schubert, Gerald] Univ Calif Los Angeles, Los Angeles, CA 90024 USA. [Tortora, Paolo] Univ Bologna, I-40126 Bologna, Italy. RP Dehant, V (reprint author), ROB, B-1180 Brussels, Belgium. EM v.dehant@oma.be RI Tortora, Paolo/J-6191-2012; Lognonne, Philippe/F-8846-2010; de Viron, Olivier/N-6647-2014 OI Tortora, Paolo/0000-0001-9259-7673; de Viron, Olivier/0000-0003-3112-9686 NR 89 TC 13 Z9 13 U1 1 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 JUL PY 2009 VL 57 IS 8-9 SI SI BP 1050 EP 1067 DI 10.1016/j.pss.2008.08.009 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 477QM UT WOS:000268533600013 ER PT J AU Biller, B Trauger, J Moody, D Close, L Kuhnert, A Stapelfeldt, K Traub, WA Kern, B AF Biller, Beth Trauger, John Moody, Dwight Close, Laird Kuhnert, Andreas Stapelfeldt, Karl Traub, Wesley A. Kern, Brian TI A Multiwavelength Differential Imaging Experiment for the High Contrast Imaging Testbed SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF THE PACIFIC LA English DT Article ID INTEGRAL FIELD SPECTROGRAPH; ADAPTIVE OPTICS; DYNAMIC-RANGE; EXTRASOLAR PLANETS; SPECKLE NOISE; YOUNG STARS; CORONAGRAPH; IMAGES; LIMITS; COMPANIONS AB We discuss the results of a multiwavelength differential imaging lab experiment with the High Contrast Imaging Testbed (HCIT) at the Jet Propulsion Laboratory. The HCIT combines a Lyot coronagraph with a Xinetics deformable mirror in a vacuum environment to simulate a space telescope in order to test technologies and algorithms for a future exoplanet coronagraph mission. At present, ground-based telescopes have achieved significant attenuation of speckle noise using the technique of spectral differential imaging (SDI). We test whether ground-based SDI can be generalized to a nonsimultaneous spectral differential imaging technique (NSDI) for a space mission. In our lab experiment, a series of five filter images centered around the O(2)(A) absorption feature at 0.762 mu m were acquired at nominal contrast values of 10(-6), 10(-7), 10(-8), and 10(-9). Outside the dark hole, single differences of images improve contrast by a factor of similar to 6. Inside the dark hole, we found significant speckle chromatism as a function of wavelength offset from the nulling wavelength, leading to a contrast degradation by a factor of 7.2 across the entire similar to 80 nm bandwidth. This effect likely stems from the chromatic behavior of the current occulter. New, less chromatic occulters are currently in development; we expect that these new occulters will resolve the speckle chromatism issue. C1 [Biller, Beth] Univ Hawaii Manoa, Inst Astron, Honolulu, HI 96822 USA. [Trauger, John; Moody, Dwight; Kuhnert, Andreas; Stapelfeldt, Karl; Traub, Wesley A.; Kern, Brian] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Close, Laird] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. RP Biller, B (reprint author), Univ Hawaii Manoa, Inst Astron, Honolulu, HI 96822 USA. RI Stapelfeldt, Karl/D-2721-2012; OI Biller, Beth/0000-0003-4614-7035 FU California Institute of Technology; NASA [NNG04GN95H, NAS 5-26555]; Space Telescope Science Institute [HST-HF-01204.01-A] FX Part of the research described in this article was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. Support for B. B. was provided by NASA through the NASA GSRP grant NNG04GN95H and the Hubble Fellowship grant HST-HF-01204.01-A awarded by the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., for NASA, under contract NAS 5-26555. NR 44 TC 4 Z9 4 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 JUL PY 2009 VL 121 IS 881 BP 716 EP 727 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 465QK UT WOS:000267601700005 ER PT J AU Goldsmith, PF Seiffert, M AF Goldsmith, Paul F. Seiffert, Michael TI A Flexible Quasioptical Input System for a Submillimeter Multiobject Spectrometer SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF THE PACIFIC LA English DT Article ID FIBER POSITIONER; NUMBER COUNTS; GALAXIES; GHZ; AMPLIFIER AB We present a conceptual design for the input optical system for a multiobject spectrometer operating at submillimeter wavelengths. The "Mirror MOS" is based on a sequence of mirrors that enables low-loss propagation of beams from selected positions distributed throughout the focal plane to the spectroscopic receiver inputs. This approach should be useful for observations of sources that have a relatively low density on the sky, for which it is inefficient to use a traditional array receiver with uniformly spaced, relatively closely packed beams. Our concept is based on assigning a patrol region to each of the receivers, which have inputs distributed over the focal plane of the telescope. The input to each receiver can be positioned at any point within this patrol region. This approach, with only four reflections, offers very low loss. The Gaussian beam optical system can be designed to produce frequency-independent illumination of the telescope, which is an important advantage for broadband systems such those required for determination of redshifts of submillimeter galaxies. C1 [Goldsmith, Paul F.; Seiffert, Michael] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Goldsmith, PF (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. RI Goldsmith, Paul/H-3159-2016 NR 24 TC 6 Z9 6 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-6280 J9 PUBL ASTRON SOC PAC JI Publ. Astron. Soc. Pac. PD JUL PY 2009 VL 121 IS 881 BP 735 EP 742 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 465QK UT WOS:000267601700007 ER PT J AU Fox, O Waczynski, A Wen, YT Foltz, RD Hill, RJ Kimble, RA Malumuth, E Rauscher, BJ AF Fox, Ori Waczynski, Augustyn Wen, Yiting Foltz, Roger D. Hill, Robert J. Kimble, Randy A. Malumuth, Eliot Rauscher, Bernard J. TI The Fe-55 X-Ray Energy Response of Mercury Cadmium Telluride Near-Infrared Detector Arrays SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF THE PACIFIC LA English DT Article ID SPACE-TELESCOPE; CALIBRATION; EFFICIENCY; HGCDTE; NOISE AB A technique involving Fe-55 X-rays provides a straightforward method to measure the response of a detector. The detector's response can lead directly to a calculation of the conversion gain (e(-)ADU(-1)), as well as aid detector design and performance studies. We calibrate the Fe-55 X-ray energy response and pair production energy of HgCdTe using 8 HST WFC3 1.7 mu m flight grade detectors. The results show that each K alpha X-ray generates 2273 +/- 137 electrons, which corresponds to a pair-production energy of 2.61 +/- 0.16 eV. The uncertainties are dominated by our knowledge of the conversion gain. In future studies, we plan to eliminate this uncertainty by directly measuring conversion gain at very low light levels. C1 [Fox, Ori] Univ Virginia, Dept Astron, Charlottesville, VA 22903 USA. [Fox, Ori; Kimble, Randy A.; Rauscher, Bernard J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Waczynski, Augustyn] Global Sci & Technol Inc, Greenbelt, MD 20771 USA. [Wen, Yiting] Muniz Engn Inc, Lanham, MD 20706 USA. [Foltz, Roger D.] Sigma Space Inc, Lanham, MD 20706 USA. [Hill, Robert J.] Conceptual Analyt LLC, Glenn Dale, MD 20769 USA. [Malumuth, Eliot] Wyle Informat Syst, Mclean, VA 22102 USA. RP Fox, O (reprint author), Univ Virginia, Dept Astron, Charlottesville, VA 22903 USA. EM ofox@virginia.edu RI Kimble, Randy/D-5317-2012 NR 19 TC 3 Z9 3 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-6280 EI 1538-3873 J9 PUBL ASTRON SOC PAC JI Publ. Astron. Soc. Pac. PD JUL PY 2009 VL 121 IS 881 BP 743 EP 754 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 465QK UT WOS:000267601700008 ER PT J AU Burke, D Gladysz, S Roberts, L Devaney, N Dainty, C AF Burke, Daniel Gladysz, Szymon Roberts, Lewis Devaney, Nicholas Dainty, Chris TI An Improved Technique for the Photometry and Astrometry of Faint Companions SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF THE PACIFIC LA English DT Article ID ADAPTIVE OPTICS PHOTOMETRY; ITERATIVE BLIND DECONVOLUTION; BINARY STARS; DIFFERENTIAL PHOTOMETRY; OBJECTIVE ASSESSMENT; SPECKLE STATISTICS; IMAGE QUALITY; SYSTEM; PLANETS; RANGE AB We propose a new approach to differential astrometry and photometry of faint companions in adaptive optics images. It is based on a prewhitening matched filter, also referred to in the literature as the Hotelling observer. We focus on cases where the signal of the companion is located within the bright halo of the parent star. Using real adaptive optics data from the 3 m Shane telescope at the Lick Observatory, we compare the performance of the Hotelling algorithm with other estimation algorithms currently used for the same problem. The real single-star data are used to generate artificial binary objects with a range of magnitude ratios. In most cases, the Hotelling observer gives significantly lower astrometric and photometric errors. In the case of high Strehl ratio (SR) data (SR approximate to 0.5), the differential photometry of a binary star with Delta m = 4.5 and a separation of 0.6 '' is better than 0.1 mag; a factor of 2 lower than the other algorithms considered. C1 [Burke, Daniel; Devaney, Nicholas; Dainty, Chris] Natl Univ Ireland, Sch Phys, Galway, Ireland. [Roberts, Lewis] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. RP Burke, D (reprint author), Natl Univ Ireland, Sch Phys, Galway, Ireland. EM daniel.burke@nuigalway.ie; sgladysz@eso.org; lewis.c.roberts@jpl.nasa.gov; nicholas.devaney@nuigalway.ie; c.dainty@nuigalway.ie FU Science Foundation Ireland [07/IN.1/I906] FX This research was funded by Science Foundation Ireland Grant No. 07/IN.1/I906. The authors wish to acknowledge the SFI/HEA Irish Centre for High-End Computing (ICHEC) for the provision of computational facilities and support. A portion of the research in this article was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. NR 42 TC 7 Z9 7 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 JUL PY 2009 VL 121 IS 881 BP 767 EP 777 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 465QK UT WOS:000267601700010 ER PT J AU Zeng, XP Tao, WK Zhang, MH Hou, AY Xie, SC Lang, S Li, XW Starr, DO Li, XF AF Zeng, Xiping Tao, Wei-Kuo Zhang, Minghua Hou, Arthur Y. Xie, Shaocheng Lang, Stephen Li, Xiaowen Starr, David O'C Li, Xiaofan TI A contribution by ice nuclei to global warming SO QUARTERLY JOURNAL OF THE ROYAL METEOROLOGICAL SOCIETY LA English DT Article DE TRMM; cloud-resolving model ID RESOLVING MODEL SIMULATIONS; CLOUD SYSTEMS; NUCLEATION PROCESSES; PROFILING ALGORITHM; CONVECTIVE CLOUD; WATER-VAPOR; MICROPHYSICS; PRECIPITATION; RADIATION; DYNAMICS AB Ice nuclei (IN) significantly affect clouds via supercooled droplets, that in turn modulate atmospheric radiation and thus climate change. Since the IN effect is relatively strong in stratiform clouds but weak in convective ones, the overall effect depends on the ratio of stratiform to convective cloud amount. In this paper, ten years of TRMM (Tropical Rainfall Measuring Mission) satellite data are analyzed to confirm that stratiform precipitation fraction increases with increasing latitude, which implies that the IN effect is stronger at higher latitudes. To quantitatively evaluate the IN effect versus latitude, large-scale forcing data from ten field campaigns are used to drive a cloud-resolving model to generate long-term cloud simulations. As revealed in the simulations, the increase in the net downward radiative flux at the top of the atmosphere from doubling the current IN concentrations is larger at higher latitude, which is attributed to the meridional tendency in the stratiform precipitation fraction. Surface warming from doubling the IN concentrations, based on the radiative balance of the globe, is compared with that from anthropogenic CO(2). It is found that the former effect is stronger than the latter in middle and high latitudes but not in the Tropics. With regard to the impact of IN on global warming, there are two factors to consider: the radiative effect from increasing the IN concentration and the increase in IN concentration itself. The former relies on cloud ensembles and thus varies mainly with latitude. In contrast, the latter relies on IN sources (e.g. the land surface distribution) and thus varies not only with latitude but also longitude. Global desertification and industrialization provide clues on the geographic variation of the increase in IN concentration since pre-industrial times. Thus, their effect on global warming can be inferred and can then be compared with observations. A general match in geographic and seasonal variations between the inferred and observed warming suggests that IN may have contributed positively to global warming over the past decades, especially in middle and high latitudes. Copyright (C) 2009 Royal Meteorological Society C1 [Zeng, Xiping; Tao, Wei-Kuo; Hou, Arthur Y.; Lang, Stephen; Li, Xiaowen; Starr, David O'C] NASA, Goddard Space Flight Ctr, Atmospheres Lab, Greenbelt, MD 20771 USA. [Zeng, Xiping; Li, Xiaowen] Univ Maryland, Goddard Earth Sci & Technol Ctr, Baltimore, MD 21201 USA. [Zhang, Minghua] SUNY Stony Brook, Sch Marine & Atmospher Sci, New York, NY USA. [Xie, Shaocheng] Lawrence Livermore Natl Lab, Div Atmospher Sci, Livermore, CA USA. [Lang, Stephen] Sci Syst & Applicat Inc, Lanham, MD USA. [Li, Xiaofan] NOAA, Natl Environm Satellite Data & Informat Serv, Camp Springs, MD USA. RP Zeng, XP (reprint author), NASA, Goddard Space Flight Ctr, Atmospheres Lab, C423,Bldg 33,Mail Code 613-1, Greenbelt, MD 20771 USA. EM zeng@agnes.gsfc.nasa.gov RI Li, Xiaofan/F-5605-2010; Hou, Arthur/D-8578-2012; Xie, Shaocheng/D-2207-2013; Li, Xiaofan/G-2094-2014 OI Xie, Shaocheng/0000-0001-8931-5145; FU NASA Headquarters Atmospheric Dynamics and Thermodynamics Program; NASA Tropical Rainfall Measuring Mission (TRMM); Office of Science (BER); US Department of Energy/Atmospheric Radiation Measurement (DOE/ARM) Interagency Agreement [DE-AI02-04ER63755]; NASA; DOE Atmospheric Radiation Measurement Program; University of California Lawrence Livermore National Laboratory [W-7405-Eng-48] FX The authors acknowledge the NASA Ames Research Center and the NASA Goddard Space Flight Center for the enormous computer time used in this research. They greatly thank Drs. Richard Johnson and Paul Ciesielski for providing the large-scale forcing data derived from NAME, TOGA-COARE and SCSMEX/SESA. Special thanks are extended to Drs. Joanne Simpson, Warren Wiscombe and three anonymous reviewers for their kind comments and suggestions. NR 72 TC 21 Z9 26 U1 0 U2 8 PU JOHN WILEY & SONS LTD PI CHICHESTER PA THE ATRIUM, SOUTHERN GATE, CHICHESTER PO19 8SQ, W SUSSEX, ENGLAND SN 0035-9009 J9 Q J ROY METEOR SOC JI Q. J. R. Meteorol. Soc. PD JUL PY 2009 VL 135 IS 643 BP 1614 EP 1629 DI 10.1002/qj.449 PG 16 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 506MI UT WOS:000270778500017 ER PT J AU Chylack, LT Peterson, LE Feiveson, AH Wear, ML Manuel, FK Tung, WH Hardy, DS Marak, LJ Cucinotta, FA AF Chylack, Leo T., Jr. Peterson, Leif E. Feiveson, Alan H. Wear, Mary L. Manuel, F. Keith Tung, William H. Hardy, Dale S. Marak, Lisa J. Cucinotta, Francis A. TI NASA Study of Cataract in Astronauts (NASCA). Report 1: Cross-Sectional Study of the Relationship of Exposure to Space Radiation and Risk of Lens Opacity SO RADIATION RESEARCH LA English DT Article ID MODELING PROPENSITY SCORES; MATRIX METALLOPROTEINASES; SERUM CAROTENOIDS; NUCLEAR CATARACT; MEDICAL-RESEARCH; TGF-BETA; TOCOPHEROLS; IRRADIATION; PRINCIPLES; REGRESSION AB The NASA Study of Cataract in Astronauts (NASCA) is a 5-year longitudinal study of the effect of space radiation exposure on the severity/progression of nuclear, cortical and posterior subcapsular (PSC) lens opacities. Here we report on baseline data that will be used over the course of the longitudinal study. Participants include 171 consenting astronauts who flew at least one mission in space and a comparison group made up of three components: (a) 53 astronauts who had not flown in space, (b) 95 military aircrew personnel, and (c) 99 non-aircrew ground-based comparison subjects. Continuous measures of nuclear, cortical and PSC lens opacities were derived from Nidek EAS 1000 digitized images. Age, demographics, general health, nutritional intake and solar ocular exposure were measured at baseline. Astronauts who flew at least one mission were matched to comparison subjects using propensity scores based on demographic characteristics and medical history stratified by gender and smoking (ever/never). The cross-sectional data for matched subjects were analyzed by fitting customized non-normal regression models to examine the effect of space radiation on each measure of opacity. The variability and median of cortical cataracts were significantly higher for exposed astronauts than for nonexposed astronauts and comparison subjects with similar ages (P = 0.015). Galactic cosmic space radiation (GCR) may be linked to increased PSC area (P = 0.056) and the number of PSC centers (P = 0.095). Within the astronaut group, PSC size was greater in subjects with higher space radiation doses (P = 0.016). No association was found between space radiation and nuclear cataracts. Cross-sectional data analysis revealed a small deleterious effect of space radiation for cortical cataracts and possibly for PSC cataracts. These results suggest increased cataract risks at smaller radiation doses than have been reported previously. (C) 2009 by Radiation Research Society C1 [Chylack, Leo T., Jr.; Tung, William H.] Brigham & Womens Hosp, Ctr Ophthalm Res, Boston, MA 02115 USA. [Peterson, Leif E.; Hardy, Dale S.] Baylor Coll Med, Dept Med, Houston, TX 77030 USA. [Peterson, Leif E.; Hardy, Dale S.] Methodist Hosp, Res Inst, Houston, TX 77030 USA. [Feiveson, Alan H.; Cucinotta, Francis A.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. [Wear, Mary L.; Marak, Lisa J.] Wyle Labs, Houston, TX USA. [Manuel, F. Keith] Space Ctr Eye Associates, Houston, TX USA. RP Chylack, LT (reprint author), Brigham & Womens Hosp, Ctr Ophthalm Res, EBRC Room 323,221 Longwood Ave, Boston, MA 02115 USA. EM ltchylack@rics.bwh.harvard.edu OI Peterson, Leif/0000-0002-1187-0883 NR 42 TC 32 Z9 34 U1 0 U2 6 PU RADIATION RESEARCH SOC PI LAWRENCE PA 810 E TENTH STREET, LAWRENCE, KS 66044 USA SN 0033-7587 J9 RADIAT RES JI Radiat. Res. PD JUL PY 2009 VL 172 IS 1 BP 10 EP 20 DI 10.1667/RR1580.1 PG 11 WC Biology; Biophysics; Radiology, Nuclear Medicine & Medical Imaging SC Life Sciences & Biomedicine - Other Topics; Biophysics; Radiology, Nuclear Medicine & Medical Imaging GA 465WF UT WOS:000267619200002 PM 19580503 ER PT J AU Abbott, BP Abbott, R Adhikari, R Ajith, P Allen, B Allen, G Amin, RS Anderson, SB Anderson, WG Arain, MA Araya, M Armandula, H Armor, P Aso, Y Aston, S Aufmuth, P Aulbert, C Babak, S Baker, P Ballmer, S Barker, C Barker, D Barr, B Barriga, P Barsotti, L Barton, MA Bartos, I Bassiri, R Bastarrika, M Behnke, B Benacquista, M Betzwieser, J Beyersdorf, PT Bilenko, IA Billingsley, G Biswas, R Black, E Blackburn, JK Blackburn, L Blair, D Bland, B Bodiya, TP Bogue, L Bork, R Boschi, V Bose, S Brady, PR Braginsky, VB Brau, JE Bridges, DO Brinkmann, M Brooks, AF Brown, DA Brummit, A Brunet, G Bullington, A Buonanno, A Burmeister, O Byer, RL Cadonati, L Camp, JB Cannizzo, J Cannon, KC Cao, J Cardenas, L Caride, S Castaldi, G Caudill, S Cavaglia, M Cepeda, C Chalermsongsak, T Chalkley, E Charlton, P Chatterji, S Chelkowski, S Chen, Y Christensen, N Chung, CTY Clark, D Clark, J Clayton, JH Cokelaer, T Colacino, CN Conte, R Cook, D Corbitt, TRC Cornish, N Coward, D Coyne, DC Creighton, JDE Creighton, TD Cruise, AM Culter, RM Cumming, A Cunningham, L Danilishin, SL Danzmann, K Daudert, B Davies, G Daw, EJ DeBra, D Degallaix, J Dergachev, V Desai, S DeSalvo, R Dhurandhar, S Diaz, M Dietz, A Donovan, F Dooley, KL Doomes, EE Drever, RP Dueck, J Duke, I Dumas, JC Dwyer, JG Echols, C Edgar, M Effler, A Ehrens, P Espinoza, E Etzel, T Evans, M Evans, T Fairhurst, S Faltas, Y Fan, Y Fazi, D Fehrmenn, H Finn, LS Flasch, K Foley, S Forrest, C Fotopoulos, N Franzen, A Frede, M Frei, M Frei, Z Freise, A Frey, R Fricke, T Fritschel, P Frolov, VV Fyffe, M Galdi, V Garofoli, JA Gholami, I Giaime, JA Giampanis, S Giardina, KD Goda, K Goetz, E Goggin, LM Gonzalez, G Gorodetsky, ML Gossler, S Gouaty, R Grant, A Gras, S Gray, C Gray, M Greenhalgh, RJS Gretarsson, AM Grimaldi, F Grosso, R Grote, H Grunewald, S Guenther, M Gustafson, EK Gustafson, R Hage, B Hallam, JM Hammer, D Hammond, GD Hanna, C Hanson, J Harms, J Harry, GM Harry, IW Harstad, ED Haughian, K Hayama, K Heefner, J Heng, IS Heptonstall, A Hewitson, M Hild, S Hirose, E Hoak, D Hodge, KA Holt, K Hosken, DJ Hough, J Hoyland, D Hughey, B Huttner, SH Ingram, DR Isogai, T Ito, M Ivanov, A Johnson, B Johnson, WW Jones, DI Jones, G Jones, R Ju, L Kalmus, P Kalogera, V Kandhasamy, S Kanner, J Kasprzyk, D Katsavounidis, E Kawabe, K Kawamura, S Kawazoe, F Kells, W Keppel, DG Khalaidovski, A Khalili, FY Khan, R Khazanov, E King, P Kissel, JS Klimenko, S Kokeyama, K Kondrashov, V Kopparapu, R Koranda, S Kozak, D Krishnan, B Kumar, R Kwee, P Lam, PK Landry, M Lantz, B Lazzarini, A Lei, H Lei, M Leindecker, N Leonor, I Li, C Lin, H Lindquist, PE Littenberg, TB Lockerbie, NA Lodhia, D Longo, M Lormand, M Lu, P Lubinski, M Lucianetti, A Luck, H Machenschalk, B MacInnis, M Mageswaran, M Mailand, K Mandel, I Mandic, V Marka, S Marka, Z Markosyan, A Markowitz, J Maros, E Martin, IW Martin, RM Marx, JN Mason, K Matichard, F Matone, L Matzner, RA Mavalvala, N McCarthy, R McClelland, DE McGuire, SC McHugh, M McIntyre, G McKechan, DJA McKenzie, K Mehmet, M Melatos, A Melissinos, AC Menendez, DF Mendell, G Mercer, RA Meshkov, S Messenger, C Meyer, MS Miller, J Minelli, J Mino, Y Mitrofanov, VP Mitselmakher, G Mittleman, R Miyakawa, O Moe, B Mohanty, SD Mohapatra, SRP Moreno, G Morioka, T Mors, K Mossavi, K MowLowry, C Mueller, G Muller-Ebhardt, H Muhammad, D Mukherjee, S Mukhopadhyay, H Mullavey, A Munch, J Murray, PG Myers, E Myers, J Nash, T Nelson, J Newton, G Nishizawa, A Numata, K O'Dell, J O'Reilly, B O'Shaughnessy, R Ochsner, E Ogin, GH Ottaway, DJ Ottens, RS Overmier, H Owen, BJ Pan, Y Pankow, C Papa, MA Parameshwaraiah, V Patel, P Pedraza, M Penn, S Perraca, A Pierro, V Pinto, IM Pitkin, M Pletsch, HJ Plissi, MV Postiglione, F Principe, M Prix, R Prokhorov, L Punken, O Quetschke, V Raab, FJ Rabeling, DS Radkins, H Raffai, P Raics, Z Rainer, N Rakhmanov, M Raymond, V Reed, CM Reed, T Rehbein, H Reid, S Reitze, DH Riesen, R Riles, K Rivera, B Roberts, P Robertson, NA Robinson, C Robinson, EL Roddy, S Rover, C Rollins, J Romano, JD Romie, JH Rowan, S Rudiger, A Russell, P Ryan, K Sakata, S de la Jordana, LS Sandberg, V Sannibale, V Santamaria, L Saraf, S Sarin, P Sathyaprakash, BS Sato, S Satterthwaite, M Saulson, PR Savage, R Savov, P Scanlan, M Schilling, R Schnabel, R Schofield, R Schulz, B Schutz, BF Schwinberg, P Scott, J Scott, SM Searle, AC Sears, B Seifert, F Sellers, D Sengupta, AS Sergeev, A Shapiro, B Shawhan, P Shoemaker, DH Sibley, A Siemens, X Sigg, D Sinha, S Sintes, AM Slagmolen, BJJ Slutsky, J Smith, JR Smith, MR Smith, ND Somiya, K Sorazu, B Stein, A Stein, LC Steplewski, S Stochino, A Stone, R Strain, KA Strigin, S Stroeer, A Stuver, AL Summerscales, TZ Sun, KX Sung, M Sutton, PJ Szokoly, GP Talukder, D Tang, L Tanner, DB Tarabrin, SP Taylor, JR Taylor, R Thacker, J Thorne, KA Thuring, A Tokmakov, KV Torres, C Torrie, C Traylor, G Trias, M Ugolini, D Ulmen, J Urbanek, K Vahlbruch, H Vallisneri, M Van den Broeck, C van der Sluys, MV van Veggel, AA Vass, S Vaulin, R Vecchio, A Veitch, J Veitch, P Veltkamp, C Villar, A Vorvick, C Vyachanin, SP Waldman, SJ Wallace, L Ward, RL Weidner, A Weinert, M Weinstein, AJ Weiss, R Wen, L Wen, S Wette, K Whelan, JT Whitcomb, SE Whiting, BF Wilkinson, C Willems, PA Williams, HR Williams, L Willke, B Wilmut, I Winkelmann, L Winkler, W Wipf, CC Wiseman, AG Woan, G Wooley, R Worden, J Wu, W Yakushin, I Yamamoto, H Yan, Z Yoshida, S Zanolin, M Zhang, J Zhang, L Zhao, C Zotov, N Zucker, ME zur Muhlen, H Zweizig, J AF Abbott, B. P. Abbott, R. Adhikari, R. Ajith, P. Allen, B. Allen, G. Amin, R. S. Anderson, S. B. Anderson, W. G. Arain, M. A. Araya, M. Armandula, H. Armor, P. Aso, Y. Aston, S. Aufmuth, P. Aulbert, C. Babak, S. Baker, P. Ballmer, S. Barker, C. Barker, D. Barr, B. Barriga, P. Barsotti, L. Barton, M. A. Bartos, I. Bassiri, R. Bastarrika, M. Behnke, B. Benacquista, M. Betzwieser, J. Beyersdorf, P. T. Bilenko, I. A. Billingsley, G. Biswas, R. Black, E. Blackburn, J. K. Blackburn, L. Blair, D. Bland, B. Bodiya, T. P. Bogue, L. Bork, R. Boschi, V. Bose, S. Brady, P. R. Braginsky, V. B. Brau, J. E. Bridges, D. O. Brinkmann, M. Brooks, A. F. Brown, D. A. Brummit, A. Brunet, G. Bullington, A. Buonanno, A. Burmeister, O. Byer, R. L. Cadonati, L. Camp, J. B. Cannizzo, J. Cannon, K. C. Cao, J. Cardenas, L. Caride, S. Castaldi, G. Caudill, S. Cavaglia, M. Cepeda, C. Chalermsongsak, T. Chalkley, E. Charlton, P. Chatterji, S. Chelkowski, S. Chen, Y. Christensen, N. Chung, C. T. Y. Clark, D. Clark, J. Clayton, J. H. Cokelaer, T. Colacino, C. N. Conte, R. Cook, D. Corbitt, T. R. C. Cornish, N. Coward, D. Coyne, D. C. Creighton, J. D. E. Creighton, T. D. Cruise, A. M. Culter, R. M. Cumming, A. Cunningham, L. Danilishin, S. L. Danzmann, K. Daudert, B. Davies, G. Daw, E. J. DeBra, D. Degallaix, J. Dergachev, V. Desai, S. DeSalvo, R. Dhurandhar, S. Diaz, M. Dietz, A. Donovan, F. Dooley, K. L. Doomes, E. E. Drever, R. W. P. Dueck, J. Duke, I. Dumas, J-C Dwyer, J. G. Echols, C. Edgar, M. Effler, A. Ehrens, P. Espinoza, E. Etzel, T. Evans, M. Evans, T. Fairhurst, S. Faltas, Y. Fan, Y. Fazi, D. Fehrmenn, H. Finn, L. S. Flasch, K. Foley, S. Forrest, C. Fotopoulos, N. Franzen, A. Frede, M. Frei, M. Frei, Z. Freise, A. Frey, R. Fricke, T. Fritschel, P. Frolov, V. V. Fyffe, M. Galdi, V. Garofoli, J. A. Gholami, I. Giaime, J. A. Giampanis, S. Giardina, K. D. Goda, K. Goetz, E. Goggin, L. M. Gonzalez, G. Gorodetsky, M. L. Gossler, S. Gouaty, R. Grant, A. Gras, S. Gray, C. Gray, M. Greenhalgh, R. J. S. Gretarsson, A. M. Grimaldi, F. Grosso, R. Grote, H. Grunewald, S. Guenther, M. Gustafson, E. K. Gustafson, R. Hage, B. Hallam, J. M. Hammer, D. Hammond, G. D. Hanna, C. Hanson, J. Harms, J. Harry, G. M. Harry, I. W. Harstad, E. D. Haughian, K. Hayama, K. Heefner, J. Heng, I. S. Heptonstall, A. Hewitson, M. Hild, S. Hirose, E. Hoak, D. Hodge, K. A. Holt, K. Hosken, D. J. Hough, J. Hoyland, D. Hughey, B. Huttner, S. H. Ingram, D. R. Isogai, T. Ito, M. Ivanov, A. Johnson, B. Johnson, W. W. Jones, D. I. Jones, G. Jones, R. Ju, L. Kalmus, P. Kalogera, V. Kandhasamy, S. Kanner, J. Kasprzyk, D. Katsavounidis, E. Kawabe, K. Kawamura, S. Kawazoe, F. Kells, W. Keppel, D. G. Khalaidovski, A. Khalili, F. Y. Khan, R. Khazanov, E. King, P. Kissel, J. S. Klimenko, S. Kokeyama, K. Kondrashov, V. Kopparapu, R. Koranda, S. Kozak, D. Krishnan, B. Kumar, R. Kwee, P. Lam, P. K. Landry, M. Lantz, B. Lazzarini, A. Lei, H. Lei, M. Leindecker, N. Leonor, I. Li, C. Lin, H. Lindquist, P. E. Littenberg, T. B. Lockerbie, N. A. Lodhia, D. Longo, M. Lormand, M. Lu, P. Lubinski, M. Lucianetti, A. Lueck, H. Machenschalk, B. MacInnis, M. Mageswaran, M. Mailand, K. Mandel, I. Mandic, V. Marka, S. Marka, Z. Markosyan, A. Markowitz, J. Maros, E. Martin, I. W. Martin, R. M. Marx, J. N. Mason, K. Matichard, F. Matone, L. Matzner, R. A. Mavalvala, N. McCarthy, R. McClelland, D. E. McGuire, S. C. McHugh, M. McIntyre, G. McKechan, D. J. A. McKenzie, K. Mehmet, M. Melatos, A. Melissinos, A. C. Menendez, D. F. Mendell, G. Mercer, R. A. Meshkov, S. Messenger, C. Meyer, M. S. Miller, J. Minelli, J. Mino, Y. Mitrofanov, V. P. Mitselmakher, G. Mittleman, R. Miyakawa, O. Moe, B. Mohanty, S. D. Mohapatra, S. R. P. Moreno, G. Morioka, T. Mors, K. Mossavi, K. MowLowry, C. Mueller, G. Mueller-Ebhardt, H. Muhammad, D. Mukherjee, S. Mukhopadhyay, H. Mullavey, A. Munch, J. Murray, P. G. Myers, E. Myers, J. Nash, T. Nelson, J. Newton, G. Nishizawa, A. Numata, K. O'Dell, J. O'Reilly, B. O'Shaughnessy, R. Ochsner, E. Ogin, G. H. Ottaway, D. J. Ottens, R. S. Overmier, H. Owen, B. J. Pan, Y. Pankow, C. Papa, M. A. Parameshwaraiah, V. Patel, P. Pedraza, M. Penn, S. Perraca, A. Pierro, V. Pinto, I. M. Pitkin, M. Pletsch, H. J. Plissi, M. V. Postiglione, F. Principe, M. Prix, R. Prokhorov, L. Punken, O. Quetschke, V. Raab, F. J. Rabeling, D. S. Radkins, H. Raffai, P. Raics, Z. Rainer, N. Rakhmanov, M. Raymond, V. Reed, C. M. Reed, T. Rehbein, H. Reid, S. Reitze, D. H. Riesen, R. Riles, K. Rivera, B. Roberts, P. Robertson, N. A. Robinson, C. Robinson, E. L. Roddy, S. Roever, C. Rollins, J. Romano, J. D. Romie, J. H. Rowan, S. Ruediger, A. Russell, P. Ryan, K. Sakata, S. Sancho de la Jordana, L. Sandberg, V. Sannibale, V. Santamaria, L. Saraf, S. Sarin, P. Sathyaprakash, B. S. Sato, S. Satterthwaite, M. Saulson, P. R. Savage, R. Savov, P. Scanlan, M. Schilling, R. Schnabel, R. Schofield, R. Schulz, B. Schutz, B. F. Schwinberg, P. Scott, J. Scott, S. M. Searle, A. C. Sears, B. Seifert, F. Sellers, D. Sengupta, A. S. Sergeev, A. Shapiro, B. Shawhan, P. Shoemaker, D. H. Sibley, A. Siemens, X. Sigg, D. Sinha, S. Sintes, A. M. Slagmolen, B. J. J. Slutsky, J. Smith, J. R. Smith, M. R. Smith, N. D. Somiya, K. Sorazu, B. Stein, A. Stein, L. C. Steplewski, S. Stochino, A. Stone, R. Strain, K. A. Strigin, S. Stroeer, A. Stuver, A. L. Summerscales, T. Z. Sun, K-X Sung, M. Sutton, P. J. Szokoly, G. P. Talukder, D. Tang, L. Tanner, D. B. Tarabrin, S. P. Taylor, J. R. Taylor, R. Thacker, J. Thorne, K. A. Thuering, A. Tokmakov, K. V. Torres, C. Torrie, C. Traylor, G. Trias, M. Ugolini, D. Ulmen, J. Urbanek, K. Vahlbruch, H. Vallisneri, M. Van den Broeck, C. van der Sluys, M. V. van Veggel, A. A. Vass, S. Vaulin, R. Vecchio, A. Veitch, J. Veitch, P. Veltkamp, C. Villar, A. Vorvick, C. Vyachanin, S. P. Waldman, S. J. Wallace, L. Ward, R. L. Weidner, A. Weinert, M. Weinstein, A. J. Weiss, R. Wen, L. Wen, S. Wette, K. Whelan, J. T. Whitcomb, S. E. Whiting, B. F. Wilkinson, C. Willems, P. A. Williams, H. R. Williams, L. Willke, B. Wilmut, I. Winkelmann, L. Winkler, W. Wipf, C. C. Wiseman, A. G. Woan, G. Wooley, R. Worden, J. Wu, W. Yakushin, I. Yamamoto, H. Yan, Z. Yoshida, S. Zanolin, M. Zhang, J. Zhang, L. Zhao, C. Zotov, N. Zucker, M. E. zur Muehlen, H. Zweizig, J. CA LIGO Sci Collaboration TI LIGO: the Laser Interferometer Gravitational-Wave Observatory SO REPORTS ON PROGRESS IN PHYSICS LA English DT Review ID ND-YAG LASER; RECYCLED MICHELSON INTERFEROMETER; FABRY-PEROT ARMS; THERMAL NOISE; OPTICAL INTERFEROMETERS; SEISMIC ISOLATION; MECHANICAL LOSS; FUSED-SILICA; DETECTORS; FREQUENCY AB The goal of the Laser Interferometric Gravitational-Wave Observatory (LIGO) is to detect and study gravitational waves (GWs) of astrophysical origin. Direct detection of GWs holds the promise of testing general relativity in the strong-field regime, of providing a new probe of exotic objects such as black holes and neutron stars and of uncovering unanticipated new astrophysics. LIGO, a joint Caltech-MIT project supported by the National Science Foundation, operates three multi-kilometer interferometers at two widely separated sites in the United States. These detectors are the result of decades of worldwide technology development, design, construction and commissioning. They are now operating at their design sensitivity, and are sensitive to gravitational wave strains smaller than one part in 10(21). With this unprecedented sensitivity, the data are being analyzed to detect or place limits on GWs from a variety of potential astrophysical sources. C1 [Abbott, B. P.; Abbott, R.; Adhikari, R.; Anderson, S. B.; Araya, M.; Armandula, H.; Aso, Y.; Ballmer, S.; Barton, M. A.; Betzwieser, J.; Billingsley, G.; Black, E.; Blackburn, J. K.; Bork, R.; Boschi, V.; Brooks, A. F.; Cannon, K. C.; Cardenas, L.; Cepeda, C.; Chalermsongsak, T.; Chatterji, S.; Coyne, D. C.; Daudert, B.; DeSalvo, R.; Echols, C.; Ehrens, P.; Espinoza, E.; Etzel, T.; Fazi, D.; Gustafson, E. K.; Hanna, C.; Heefner, J.; Heptonstall, A.; Hodge, K. A.; Ivanov, A.; Kalmus, P.; Kells, W.; Keppel, D. G.; King, P.; Kondrashov, V.; Kozak, D.; Lazzarini, A.; Lei, M.; Lindquist, P. E.; Mageswaran, M.; Mailand, K.; Maros, E.; Marx, J. N.; McIntyre, G.; Meshkov, S.; Miyakawa, O.; Nash, T.; Ogin, G. H.; Patel, P.; Pedraza, M.; Robertson, N. A.; Russell, P.; Sannibale, V.; Searle, A. C.; Sears, B.; Sengupta, A. S.; Smith, M. R.; Stochino, A.; Taylor, R.; Torrie, C.; Vass, S.; Villar, A.; Wallace, L.; Ward, R. L.; Weinstein, A. J.; Whitcomb, S. E.; Willems, P. A.; Yamamoto, H.; Zhang, L.; Zweizig, J.] CALTECH, LIGO, Pasadena, CA 91125 USA. [Ajith, P.; Allen, B.; Aulbert, C.; Brinkmann, M.; Burmeister, O.; Danzmann, K.; Degallaix, J.; Dueck, J.; Fehrmenn, H.; Frede, M.; Giampanis, S.; Gossler, S.; Grote, H.; Hewitson, M.; Kawazoe, F.; Khalaidovski, A.; Lueck, H.; Mehmet, M.; Messenger, C.; Mors, K.; Mossavi, K.; Mueller-Ebhardt, H.; Pletsch, H. J.; Prix, R.; Punken, O.; Rainer, N.; Rehbein, H.; Roever, C.; Ruediger, A.; Schilling, R.; Schnabel, R.; Schulz, B.; Seifert, F.; Taylor, J. R.; Veltkamp, C.; Weidner, A.; Weinert, M.; Willke, B.; Winkelmann, L.; Winkler, W.] Max Planck Inst Gravitat Phys, Albert Einstein Inst, D-30167 Hannover, Germany. [Allen, B.; Anderson, W. G.; Armor, P.; Biswas, R.; Brady, P. R.; Clayton, J. H.; Creighton, J. D. E.; Flasch, K.; Fotopoulos, N.; Goggin, L. M.; Hammer, D.; Koranda, S.; Mercer, R. A.; Moe, B.; Papa, M. A.; Siemens, X.; Vaulin, R.; Wiseman, A. G.] Univ Wisconsin, Dept Phys, Milwaukee, WI 53201 USA. [Allen, G.; Bullington, A.; Byer, R. L.; Clark, D.; DeBra, D.; Lantz, B.; Leindecker, N.; Lu, P.; Markosyan, A.; Sinha, S.; Sun, K-X; Ulmen, J.; Urbanek, K.] Stanford Univ, EL Lab, Stanford, CA 94305 USA. [Amin, R. S.; Caudill, S.; Giaime, J. A.; Gonzalez, G.; Gouaty, R.; Johnson, W. W.; Kissel, J. S.; Matichard, F.; Slutsky, J.; Sung, M.; Wen, S.] Louisiana State Univ, Dept Phys & Astron, Baton Rouge, LA 70803 USA. [Arain, M. A.; Dooley, K. L.; Faltas, Y.; Klimenko, S.; Lei, H.; Lin, H.; Lucianetti, A.; Martin, R. M.; Mitselmakher, G.; Mueller, G.; Ottens, R. S.; Pankow, C.; Quetschke, V.; Reitze, D. H.; Tanner, D. B.; Whiting, B. F.; Williams, L.; Wu, W.] Univ Florida, Dept Phys, Gainesville, FL 32611 USA. [Aston, S.; Chelkowski, S.; Cruise, A. M.; Culter, R. M.; Freise, A.; Hallam, J. M.; Hild, S.; Kasprzyk, D.; Lodhia, D.; Perraca, A.; Vecchio, A.; Veitch, J.] Univ Birmingham, Sch Phys & Astron, Birmingham B15 2TT, W Midlands, England. [Aufmuth, P.; Danzmann, K.; Franzen, A.; Hage, B.; Kwee, P.; Lueck, H.; Thuering, A.; Vahlbruch, H.; Willke, B.; zur Muehlen, H.] Leibniz Univ Hannover, Inst Gravitat Phys, D-30167 Hannover, Germany. [Babak, S.; Behnke, B.; Chen, Y.; Gholami, I.; Grunewald, S.; Krishnan, B.; Machenschalk, B.; Papa, M. A.; Robinson, E. L.; Santamaria, L.; Schutz, B. F.; Whelan, J. T.] Max Planck Inst Gravitat Phys, Albert Einstein Inst, D-14476 Golm, Germany. [Baker, P.; Cornish, N.; Littenberg, T. B.] Montana State Univ, Dept Phys, Bozeman, MT 59717 USA. [Barker, C.; Barker, D.; Bland, B.; Cook, D.; Effler, A.; Gray, C.; Guenther, M.; Ingram, D. R.; Johnson, B.; Kawabe, K.; Landry, M.; Lubinski, M.; McCarthy, R.; Mendell, G.; Moreno, G.; Myers, E.; Myers, J.; Parameshwaraiah, V.; Raab, F. J.; Radkins, H.; Reed, C. M.; Rivera, B.; Ryan, K.; Sandberg, V.; Savage, R.; Schwinberg, P.; Sigg, D.; Vorvick, C.; Wilkinson, C.; Worden, J.] Hanford Observ, LIGO, Richland, WA 99352 USA. [Barr, B.; Bassiri, R.; Bastarrika, M.; Chalkley, E.; Cumming, A.; Cunningham, L.; Edgar, M.; Grant, A.; Hammond, G. D.; Haughian, K.; Heng, I. S.; Hough, J.; Huttner, S. H.; Jones, R.; Kumar, R.; Martin, I. W.; Miller, J.; Murray, P. G.; Nelson, J.; Newton, G.; Pitkin, M.; Plissi, M. V.; Reid, S.; Robertson, N. A.; Rowan, S.; Scott, J.; Sorazu, B.; Strain, K. A.; Tokmakov, K. V.; van Veggel, A. A.; Woan, G.] Univ Glasgow, Dept Phys & Astron, Glasgow G12 8QQ, Lanark, Scotland. [Barriga, P.; Blair, D.; Coward, D.; Dumas, J-C; Fan, Y.; Gras, S.; Hoyland, D.; Ju, L.; Wen, L.; Yan, Z.; Zhao, C.] Univ Western Australia, Sch Phys, Crawley, WA 6009, Australia. [Barsotti, L.; Blackburn, L.; Bodiya, T. P.; Brunet, G.; Cao, J.; Corbitt, T. R. C.; Donovan, F.; Duke, I.; Evans, M.; Foley, S.; Fritschel, P.; Goda, K.; Grimaldi, F.; Harry, G. M.; Hughey, B.; Katsavounidis, E.; MacInnis, M.; Markowitz, J.; Mason, K.; Mavalvala, N.; Mittleman, R.; Sarin, P.; Shapiro, B.; Shoemaker, D. H.; Smith, N. D.; Stein, A.; Stein, L. C.; Waldman, S. J.; Weiss, R.; Wipf, C. C.; Zucker, M. E.] MIT, LIGO, Cambridge, MA 02139 USA. [Bartos, I.; Dwyer, J. G.; Khan, R.; Marka, S.; Marka, Z.; Raics, Z.; Rollins, J.] Columbia Univ, Dept Phys, New York, NY 10027 USA. [Benacquista, M.; Creighton, T. D.; Diaz, M.; Grosso, R.; Hayama, K.; Mohanty, S. D.; Mukherjee, S.; Rakhmanov, M.; Romano, J. D.; Stone, R.; Tang, L.] Univ Texas Brownsville & Texas Southmost Coll, Dept Phys, Brownsville, TX 78520 USA. [Beyersdorf, P. T.] San Jose State Univ, Dept Phys & Astron, San Jose, CA 95192 USA. [Bilenko, I. A.; Braginsky, V. B.; Danilishin, S. L.; Gorodetsky, M. L.; Khalili, F. Y.; Mitrofanov, V. P.; Prokhorov, L.; Strigin, S.; Tarabrin, S. P.; Vyachanin, S. P.] Moscow MV Lomonosov State Univ, Relat Grp, Moscow 119992, Russia. [Bogue, L.; Bridges, D. O.; Evans, T.; Fricke, T.; Frolov, V. V.; Fyffe, M.; Giaime, J. A.; Giardina, K. D.; Hanson, J.; Hoak, D.; Holt, K.; Lormand, M.; Meyer, M. S.; Muhammad, D.; O'Reilly, B.; Overmier, H.; Riesen, R.; Roddy, S.; Romie, J. H.; Sellers, D.; Sibley, A.; Stuver, A. L.; Thacker, J.; Thorne, K. A.; Torres, C.; Traylor, G.; Wooley, R.; Yakushin, I.] Livingston Observ, LIGO, Livingston, LA 70754 USA. 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M.; Principe, M.] Univ Sannio Benevento, Dept Engn, I-82100 Benevento, Italy. [Cavaglia, M.] Univ Mississippi, Dept Phys & Astron, University, MS 38677 USA. [Charlton, P.] Charles Sturt Univ, Res Scool Phys & Engn, Wagga Wagga, NSW 2678, Australia. [Chen, Y.; Li, C.; Mino, Y.; Savov, P.; Somiya, K.; Vallisneri, M.; Wen, L.] CALTECH, CaRT, Pasadena, CA 91125 USA. [Christensen, N.; Isogai, T.] Carleton Coll, Dept Phys & Astron, Northfield, MN 55057 USA. [Chung, C. T. Y.; Melatos, A.] Univ Melbourne, Sch Phys, Parkville, Vic 3010, Australia. [Clark, J.; Cokelaer, T.; Davies, G.; Dietz, A.; Fairhurst, S.; Harry, I. W.; Jones, G.; McKechan, D. J. A.; Robinson, C.; Sathyaprakash, B. S.; Schutz, B. F.; Sutton, P. J.; Van den Broeck, C.] Cardiff Univ, Sch Phys & Astron, Cardiff CF24 3AA, S Glam, Wales. [Colacino, C. N.; Frei, Z.; Raffai, P.; Szokoly, G. P.] Eotvos Lorand Univ, Inst Phys, ELTE, H-1053 Budapest, Hungary. [Conte, R.; Postiglione, F.] Univ Salerno, Dept Phys, I-84084 Salerno, Italy. [Daw, E. J.] Univ Sheffield, Dept Phys & Astron, Sheffield S10 2TN, S Yorkshire, England. [Desai, S.; Finn, L. S.; Kopparapu, R.; Menendez, D. F.; Minelli, J.; O'Shaughnessy, R.; Owen, B. J.; Williams, H. R.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Dhurandhar, S.; Mukhopadhyay, H.] Interuniv Ctr Astron & Astrophys, Pune 411007, Maharashtra, India. [Doomes, E. E.; McGuire, S. C.] Southern Univ, Dept Phys, Baton Rouge, LA 70813 USA. [Doomes, E. E.; McGuire, S. C.] A&M Coll, Baton Rouge, LA 70813 USA. [Forrest, C.; Melissinos, A. C.] Univ Rochester, Dept Phys & Astron, Rochester, NY 14627 USA. [Frei, M.; Matzner, R. A.] Univ Texas Austin, Dept Phys, Austin, TX 78712 USA. [Gray, M.; Lam, P. K.; McClelland, D. E.; McKenzie, K.; MowLowry, C.; Mullavey, A.; Rabeling, D. S.; Satterthwaite, M.; Scott, S. M.; Slagmolen, B. J. J.; Wette, K.] Australian Natl Univ, Res Sch Phys & Engn, Canberra, ACT 0200, Australia. [Gretarsson, A. M.; Zanolin, M.] Embry Riddle Aeronaut Univ, Dept Phys, Prescott, AZ 86301 USA. [Harms, J.; Kandhasamy, S.; Mandic, V.] Univ Minnesota, Dept Phys, Minneapolis, MN 55455 USA. [Hosken, D. J.; Munch, J.; Ottaway, D. J.; Veitch, P.] Univ Adelaide, Sch Chem & Phys, Adelaide, SA 5005, Australia. [Jones, D. I.] Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England. [Kalogera, V.; Mandel, I.; Raymond, V.; van der Sluys, M. V.] Northwestern Univ, Dept Astron & Astrophys, Evanston, IL 60208 USA. [Kawamura, S.; Kokeyama, K.; Morioka, T.; Nishizawa, A.; Sakata, S.; Sato, S.] Natl Astron Observ Japan, Tokyo 1818588, Japan. [Khazanov, E.; Sergeev, A.] Inst Appl Phys, Nizhnii Novgorod 603950, Russia. [Lockerbie, N. A.] Univ Strathclyde, Dept Phys, Glasgow G1 1XQ, Lanark, Scotland. [McHugh, M.] Loyola Univ, Dept Phys, New Orleans, LA 70118 USA. [Penn, S.] Hobart & William Smith Coll, Geneva, NY 14456 USA. [Reed, T.; Scanlan, M.; Zotov, N.] Louisiana Tech Univ, Dept Phys, Ruston, LA 71272 USA. [Roberts, P.; Summerscales, T. Z.] Andrews Univ, Dept Phys, Berrien Springs, MI 49104 USA. [Sancho de la Jordana, L.; Sintes, A. M.; Trias, M.] Univ Illes Balears, Relat & Gravitat Grp, E-07122 Palma de Mallorca, Spain. [Saraf, S.] Sonoma State Univ, Dept Phys & Astron, Rohnert Pk, CA 94928 USA. [Ugolini, D.] Trinity Univ, Dept Phys & Astron, San Antonio, TX 78212 USA. [Whelan, J. T.] Rochester Inst Technol, Rochester, NY 14623 USA. [Yoshida, S.] SE Louisiana Univ, Hammond, LA 70402 USA. RP Abbott, BP (reprint author), CALTECH, LIGO, Pasadena, CA 91125 USA. EM peter.fritschel@ligo.org RI Hammond, Giles/B-7861-2009; McClelland, David/E-6765-2010; Hild, Stefan/A-3864-2010; Schutz, Bernard/B-1504-2010; Rowan, Sheila/E-3032-2010; Galdi, Vincenzo/B-1670-2008; Strain, Kenneth/D-5236-2011; Raab, Frederick/E-2222-2011; Martin, Iain/A-2445-2010; Lueck, Harald/F-7100-2011; Kawazoe, Fumiko/F-7700-2011; Freise, Andreas/F-8892-2011; Lam, Ping Koy/A-5276-2008; Kawabe, Keita/G-9840-2011; Biswas, Rahul/H-7474-2016; Harms, Jan/J-4359-2012; Bartos, Imre/A-2592-2017; Frey, Raymond/E-2830-2016; Sergeev, Alexander/F-3027-2017; Ward, Robert/I-8032-2014; Pitkin, Matthew/I-3802-2013; Vyatchanin, Sergey/J-2238-2012; Khazanov, Efim/B-6643-2014; Lucianetti, Antonio/G-7383-2014; Danilishin, Stefan/K-7262-2012; Khalili, Farit/D-8113-2012; Vecchio, Alberto/F-8310-2015; Mow-Lowry, Conor/F-8843-2015; Khan, Rubab/F-9455-2015; Ottaway, David/J-5908-2015; Postiglione, Fabio/O-4744-2015; Sigg, Daniel/I-4308-2015; Pinto, Innocenzo/L-3520-2016; Hammond, Giles/A-8168-2012; Finn, Lee Samuel/A-3452-2009; Santamaria, Lucia/A-7269-2012; Prokhorov, Leonid/I-2953-2012; Gorodetsky, Michael/C-5938-2008; Strigin, Sergey/I-8337-2012; 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 McClelland, David/0000-0001-6210-5842; Galdi, Vincenzo/0000-0002-4796-3600; Strain, Kenneth/0000-0002-2066-5355; Lueck, Harald/0000-0001-9350-4846; Lam, Ping Koy/0000-0002-4421-601X; Papa, M.Alessandra/0000-0002-1007-5298; Kanner, Jonah/0000-0001-8115-0577; Aulbert, Carsten/0000-0002-1481-8319; Scott, Jamie/0000-0001-6701-6515; Freise, Andreas/0000-0001-6586-9901; Mandel, Ilya/0000-0002-6134-8946; Whiting, Bernard F/0000-0002-8501-8669; Veitch, John/0000-0002-6508-0713; Principe, Maria/0000-0002-6327-0628; Boschi, Valerio/0000-0001-8665-2293; Matichard, Fabrice/0000-0001-8982-8418; Pinto, Innocenzo M./0000-0002-2679-4457; Minelli, Jeff/0000-0002-5330-912X; Santamaria, Lucia/0000-0002-5986-0449; Pierro, Vincenzo/0000-0002-6020-5521; Hallam, Jonathan Mark/0000-0002-7087-0461; Biswas, Rahul/0000-0002-0774-8906; Sorazu, Borja/0000-0002-6178-3198; Nishizawa, Atsushi/0000-0003-3562-0990; Zweizig, John/0000-0002-1521-3397; O'Shaughnessy, Richard/0000-0001-5832-8517; Frey, Raymond/0000-0003-0341-2636; Stein, Leo/0000-0001-7559-9597; Ward, Robert/0000-0001-5503-5241; Whelan, John/0000-0001-5710-6576; LONGO, Maurizio/0000-0001-8325-4003; Fairhurst, Stephen/0000-0001-8480-1961; Pitkin, Matthew/0000-0003-4548-526X; Danilishin, Stefan/0000-0001-7758-7493; Vecchio, Alberto/0000-0002-6254-1617; Khan, Rubab/0000-0001-5100-5168; Postiglione, Fabio/0000-0003-0628-3796; Sigg, Daniel/0000-0003-4606-6526; Finn, Lee Samuel/0000-0002-3937-0688; Gorodetsky, Michael/0000-0002-5159-2742; Allen, Bruce/0000-0003-4285-6256; Zhao, Chunnong/0000-0001-5825-2401; FU United States National Science Foundation; LIGO Laboratory; Particle Physics and Astronomy Research Council of the UK; Max-Planck-Society; State of Niedersachsen/Germany; Australian Research Council; Natural Sciences and Engineering Research Council of Canada; Council of Scientific and Industrial Research of India; Department of Science and Technology of India; Spanish Ministerio de Educacion y Ciencia; National Aeronautics and Space Administration; John Simon Guggenheim Foundation; Alexander von Humboldt Foundation; Leverhulme Trust; David and Lucile Packard Foundation; Research Corporation; Alfred P Sloan Foundation FX The authors gratefully acknowledge the support of the United States National Science Foundation for the construction and operation of the LIGO Laboratory and the Particle Physics and Astronomy Research Council of the UK, the Max-Planck-Society and the State of Niedersachsen/Germany for support of the construction and operation of the GEO600 detector. The authors also gratefully acknowledge the support of the research by these agencies and by the Australian Research Council, the Natural Sciences and Engineering Research Council of Canada, the Council of Scientific and Industrial Research of India, the Department of Science and Technology of India, the Spanish Ministerio de Educacion y Ciencia, The National Aeronautics and Space Administration, the John Simon Guggenheim Foundation, the Alexander von Humboldt Foundation, the Leverhulme Trust, the David and Lucile Packard Foundation, the Research Corporation and the Alfred P Sloan Foundation. NR 102 TC 634 Z9 641 U1 47 U2 170 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0034-4885 EI 1361-6633 J9 REP PROG PHYS JI Rep. Prog. Phys. PD JUL PY 2009 VL 72 IS 7 AR 076901 DI 10.1088/0034-4885/72/7/076901 PG 25 WC Physics, Multidisciplinary SC Physics GA 464NG UT WOS:000267511200004 ER PT J AU Schmitt, HH AF Schmitt, Harrison H. TI From the Moon to Mars SO SCIENTIFIC AMERICAN LA English DT Article C1 [Schmitt, Harrison H.] Harvard Univ, Cambridge, MA 02138 USA. [Schmitt, Harrison H.] US Geol Survey, Reston, VA USA. [Schmitt, Harrison H.] Univ Wisconsin, Madison, WI USA. [Schmitt, Harrison H.] NASA, Advisory Council, Washington, DC USA. RP Schmitt, HH (reprint author), Harvard Univ, Cambridge, MA 02138 USA. NR 0 TC 3 Z9 3 U1 0 U2 1 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 JUL PY 2009 VL 301 IS 1 BP 36 EP 43 PG 8 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 460PF UT WOS:000267198900031 PM 19555022 ER PT J AU Higinbotham, JR Moisan, JR Orton, PM AF Higinbotham, John R. Moisan, John R. Orton, Philip M. TI Solar Powered Autonomous Surface Vehicle Development and Operation SO SEA TECHNOLOGY LA English DT Article C1 [Higinbotham, John R.] Emergent Space Technol Inc, Autonomous Vehicles Grp, Greenbelt, MD USA. [Moisan, John R.] NASA, Goddard Space Flight Ctr, Wallops Flight Facil, Wallops Isl, VA 23337 USA. [Orton, Philip M.] Columbia Univ, Lamont Doherty Geol Observ, Palisades, NY 10964 USA. RP Higinbotham, JR (reprint author), Emergent Space Technol Inc, Autonomous Vehicles Grp, Greenbelt, MD USA. EM john.higinbotham@emergentspace.com RI Orton, Philip/A-9791-2010 FU NOAA [NA03NOS4730220]; NASA/GSFC FX The authors would like to acknowledge NOAA, which funded this work under award NA03NOS4730220. The statements, findings, conclusions and recommendations contained in this article are those of the authors and do not necessarily reflect the views of NOAA or the U.S. Department of Commerce. Support for Moisan was provided by NASA/GSFC. The authors would also like to acknowledge Dr. Wade McGillis of Lamont-Doherty Earth Observatory. NR 0 TC 0 Z9 0 U1 0 U2 2 PU COMPASS PUBLICATIONS, INC PI ARLINGTON PA 1501 WILSON BLVD., STE 1001, ARLINGTON, VA 22209-2403 USA SN 0093-3651 J9 SEA TECHNOL JI Sea Technol. PD JUL PY 2009 VL 50 IS 7 BP 10 EP 13 PG 4 WC Engineering, Ocean SC Engineering GA 476FZ UT WOS:000268425400002 ER PT J AU Wang, TS AF Wang, Ten-See TI Transient three-dimensional startup side load analysis of a regeneratively cooled nozzle SO SHOCK WAVES LA English DT Article DE Transient nozzle side loads; Regeneratively cooled nozzle; Shock pulsation; Shock transition; Combustion wave; Coanda effect ID HEAT-TRANSFER; FLOWS; PERFORMANCE AB The objective of this effort is to develop a computational methodology to capture the side load physics and to anchor the computed aerodynamic side loads with the available data by simulating the startup transient of a regeneratively cooled, high-aspect-ratio nozzle, hot-fired at sea level. The computational methodology is based on an unstructured-grid, pressure-based, reacting flow computational fluid dynamics and heat transfer formulation, and a transient inlet history based on an engine system simulation. Emphases were put on the effects of regenerative cooling on shock formation inside the nozzle, and ramp rate on side load reduction. The results show that three types of asymmetric shock physics incur strong side loads: the generation of combustion wave, shock transitions, and shock pulsations across the nozzle lip, albeit the combustion wave can be avoided with sparklers during hot-firing. Results from both regenerative cooled and adiabatic wall boundary conditions capture the early shock transitions with corresponding side loads matching the measured secondary side load. It is theorized that the first transition from free-shock separation to restricted-shock separation is caused by the Coanda effect. After which the regeneratively cooled wall enhances the Coanda effect such that the supersonic jet stays attached, while the hot adiabatic wall fights off the Coanda effect, and the supersonic jet becomes detached most of the time. As a result, the computed peak side load and dominant frequency due to shock pulsation across the nozzle lip associated with the regeneratively cooled wall boundary condition match those of the test, while those associated with the adiabatic wall boundary condition are much too low. Moreover, shorter ramp time results show that higher ramp rate has the potential in reducing the nozzle side loads. C1 NASA, George C Marshall Space Flight Ctr, Fluid Dynam Branch, Huntsville, AL 35812 USA. RP Wang, TS (reprint author), NASA, George C Marshall Space Flight Ctr, Fluid Dynam Branch, Huntsville, AL 35812 USA. EM Ten-See.Wang-1@nasa.gov NR 28 TC 19 Z9 21 U1 2 U2 5 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0938-1287 J9 SHOCK WAVES JI Shock Waves PD JUL PY 2009 VL 19 IS 3 BP 251 EP 264 DI 10.1007/s00193-009-0201-2 PG 14 WC Mechanics SC Mechanics GA 457RW UT WOS:000266951600008 ER PT J AU Xapsos, MA Burke, EA AF Xapsos, M. A. Burke, E. A. TI Evidence of 6 000-Year Periodicity in Reconstructed Sunspot Numbers SO SOLAR PHYSICS LA English DT Article DE Solar activity, periodic; Hurst analysis; Smoothing filter; Fourier analysis ID SERIES AB Reconstructed sunspot data are available that extend solar activity back to 11 360 years before the present. We have examined these data using Hurst analysis, a moving average filter, and Fourier analysis. All of the procedures indicate the presence of a long term (a parts per thousand 6 000 year) cycle not previously reported. A number of shorter cycles formerly identified in the literature by using Fourier analysis, Bayes methods, and maximum entropy methods were also detected in the reconstructed sunspot data. C1 [Xapsos, M. A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Xapsos, MA (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. EM Michael.A.Xapsos@nasa.gov NR 16 TC 10 Z9 11 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 JUL PY 2009 VL 257 IS 2 BP 363 EP 369 DI 10.1007/s11207-009-9380-3 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 459NX UT WOS:000267111100011 ER PT J AU Malick, MJ Adkison, MD Wertheimer, AC AF Malick, Michael J. Adkison, Milo D. Wertheimer, Alex C. TI Variable Effects of Biological and Environmental Processes on Coho Salmon Marine Survival in Southeast Alaska SO TRANSACTIONS OF THE AMERICAN FISHERIES SOCIETY LA English DT Article ID NORTHEAST PACIFIC SALMON; OREGON PRODUCTION AREA; JUVENILE CHUM SALMON; ONCORHYNCHUS-KISUTCH; BRITISH-COLUMBIA; PINK SALMON; SOCKEYE-SALMON; OCEAN GROWTH; EMBRYO SURVIVAL; FRASER-RIVER AB Correlation analyses, linear regression models, and multistock mixed effects models were used to examine the relationships between coho salmon Oncorhynchus kisutch marine survival and six biological and environmental covariates across 14 southeast Alaska (SEAK) stocks. A primary focus of the study was to investigate the influence of pink salmon O. gorbuscha and chum salmon O. keta fry abundances on coho salmon marine survival. The coho salmon stocks exhibited strong covariation; 88 of the 91 pairwise comparisons among the coho salmon stocks covaried positively and 54 of them were significant (P < 0.05). Only one of the covariates, the North Pacific index, which is a measure of the Aleutian low pressure zone, had consistent relationships (positive) across all 14 stocks. The other covariates, including freshwater discharge, the Pacific decadal oscillation, sea-surface temperature, and two indices of pink salmon and chum salmon fry abundances, all had inconsistent relationships with marine survival. The best-fit linear regression models varied greatly among the 14 stocks, as did the R(2) values, which ranged from 0.00 to 0.54. An index representing local hatchery pink salmon and chum salmon fry abundance was the most important variable in explaining the variation in marine survival, having a stronger estimated effect on survival than an index of local wild pink salmon fry abundance. The magnitude and sign of the hatchery pink salmon and chum salmon effect varied greatly among different localities. Our results suggest that (1) SEAK coho salmon stocks are not equally influenced by the same factors and (2) there are factors that appear to affect marine survival of SEAK coho salmon stocks at varying spatial scales. This study also provides evidence that coho salmon stocks throughout SEAK experience some degree of regional concordance in the marine environment but also that local stock-specific conditions are important in fully understanding variation in marine survival. C1 [Malick, Michael J.] Univ Alaska Fairbanks, Sch Fisheries & Ocean Sci, Juneau Ctr, Juneau, AK 99801 USA. [Adkison, Milo D.] Univ Alaska Fairbanks, Sch Fisheries & Ocean Sci, Fairbanks, AK 99775 USA. [Wertheimer, Alex C.] Ted Stevens Marine Res Inst, Auke Bay Labs, Natl Marine Fisheries Serv, Juneau, AK 99801 USA. RP Malick, MJ (reprint author), Univ Alaska Fairbanks, Sch Fisheries & Ocean Sci, Juneau Ctr, 17101 Point Lena Loop Rd, Juneau, AK 99801 USA. EM mjmalick@alaska.edu FU U.S. Global Ocean Ecosystem Dynamics FX Funding for this research was provided by the U.S. Global Ocean Ecosystem Dynamics research program through the National Science Foundation. We thank L. Shaul, C. Blair, G. Freitag, R. Focht, X. Zhang, M. Plotnick, S. Heinl, and T. Royer for graciously providing auxiliary data. We also thank N. Hillgruber, B. Smoker, and two anonymous reviewers for comments on early manuscripts. NR 63 TC 5 Z9 5 U1 1 U2 6 PU AMER FISHERIES SOC PI BETHESDA PA 5410 GROSVENOR LANE SUITE 110, BETHESDA, MD 20814-2199 USA SN 0002-8487 J9 T AM FISH SOC JI Trans. Am. Fish. Soc. PD JUL PY 2009 VL 138 IS 4 BP 846 EP 860 DI 10.1577/T08-177.1 PG 15 WC Fisheries SC Fisheries GA 477EL UT WOS:000268501300013 ER PT J AU DellaCorte, C AF DellaCorte, Christopher TI A blue moon for tribology SO TRIBOLOGY & LUBRICATION TECHNOLOGY LA English DT Editorial Material C1 NASA, Glenn Res Ctr, Cleveland, OH USA. RP DellaCorte, C (reprint author), NASA, Glenn Res Ctr, Cleveland, OH USA. EM christopher.dellacorte@nasa.gov NR 0 TC 0 Z9 0 U1 0 U2 0 PU SOC TRIBOLOGISTS & LUBRICATION ENGINEERS PI PARK RIDGE PA 840 BUSSE HIGHWAY, PARK RIDGE, IL 60068 USA SN 1545-858X J9 TRIBOL LUBR TECHNOL JI Tribol. Lubr. Technol. PD JUL PY 2009 VL 65 IS 7 BP 26 EP 27 PG 2 WC Engineering, Mechanical SC Engineering GA 472JZ UT WOS:000268128200006 ER PT J AU Jones, JA Sargsyan, AE Barr, YR Melton, S Hamilton, DR Dulchavsky, SA Whitson, PA AF Jones, J. A. Sargsyan, A. E. Barr, Y. R. Melton, S. Hamilton, D. R. Dulchavsky, S. A. Whitson, P. A. TI DIAGNOSTIC ULTRASOUND AT MACH 20: RETROPERITONEAL AND PELVIC IMAGING IN SPACE SO ULTRASOUND IN MEDICINE AND BIOLOGY LA English DT Article DE Ultrasound; Retroperitoneal imaging; Astronaut; Microgravity; Spaceflight; International space station ID MICROGRAVITY; SPACEFLIGHT; ASTRONAUTS; STATION; ABOARD AB An operationally available diagnostic imaging capability augments spaceflight medical support by facilitating the diagnosis, monitoring and treatment of medical or surgical conditions, by improving medical outcomes and, thereby, by lowering medical mission impacts and the probability of crew evacuation due to medical causes. Microgravity-related physiological changes occurring during spaceflight can affect the genitourinary system and potentially cause conditions such as urinary retention or nephrolithiasis for which ultrasonography (U/S) would he a useful diagnostic tool. This study describes the first genitourinary ultrasound examination conducted in space, and evaluates image quality, frame rate, resolution requirements, real-time remote guidance of nonphysician crew medical officers and evaluation of on-orbit tools that can augment image acquisition. A nonphysician crew medical officer (CMO) astronaut, with minimal training in U/S, performed a self-examination of the genitourinary system onboard the International Space Station, using a Philips/ATL Model HDI-5000 ultrasound imaging unit located in the International Space Station Human Research Facility. The CMO was remotely guided by voice commands from experienced, earth-based sonographers stationed in Mission Control Center in Houston. The crewmember, with guidance, was able to acquire all of the target images. Real-time and still U/S images received at Mission Control Center in Houston were of sufficient quality for the images to be diagnostic for multiple potential genitourinary applications. Microgravity-based ultrasound imaging can provide diagnostic quality images of the retroperitoneum and pelvis, offering improved diagnosis and treatment for onboard medical contingencies. Successful completion of complex sonographic examinations can be obtained even with minimally trained nonphysician ultrasound operators, with the assistance of ground-based real-time guidance. (E-mail: jeffrey.a.jones@nasa.gov) Published by Elsevier Inc. on behalf of World Federation for Ultrasound in Medicine & Biology. C1 [Jones, J. A.] NASA, Lyndon B Johnson Space Ctr, JSC SD2, Space Med & Hlth Care Syst Med Operat Branch, Houston, TX 77058 USA. [Jones, J. A.] Int Space Univ, Strasbourg, France. [Sargsyan, A. E.; Melton, S.; Hamilton, D. R.] Wyle Integrated Sci & Engn Grp, Houston, TX USA. [Barr, Y. R.] Univ Texas Med Branch, Dept Prevent Med Aerosp Med, Galveston, TX USA. [Dulchavsky, S. A.] Henry Ford Hosp, Dept Surg, Detroit, MI 48202 USA. RP Jones, JA (reprint author), NASA, Lyndon B Johnson Space Ctr, JSC SD2, Space Med & Hlth Care Syst Med Operat Branch, 2101 NASA Pkwy, Houston, TX 77058 USA. EM jeffrey.a.jones@nasa.gov NR 14 TC 8 Z9 8 U1 2 U2 6 PU ELSEVIER SCIENCE INC PI NEW YORK PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA SN 0301-5629 J9 ULTRASOUND MED BIOL JI Ultrasound Med. Biol. PD JUL PY 2009 VL 35 IS 7 BP 1059 EP 1067 DI 10.1016/j.ultrasmedbio.2009.01.002 PG 9 WC Acoustics; Radiology, Nuclear Medicine & Medical Imaging SC Acoustics; Radiology, Nuclear Medicine & Medical Imaging GA 470EB UT WOS:000267956300001 PM 19427106 ER PT J AU Wohl, CJ Belcher, MA Ghose, S Connell, JW AF Wohl, Christopher J. Belcher, Marcus A. Ghose, Sayata Connell, John W. TI Modification of the surface properties of polyimide films using polyhedral oligomeric silsesquioxane deposition and oxygen plasma exposure SO APPLIED SURFACE SCIENCE LA English DT Article DE Polyimide; Polyhedral oligomeric silsesquioxane; Oxygen plasma; Lunar dust ID ATOMIC-OXYGEN; SILOXANE COPOLYMERS; CONTACT ANGLES; LUNAR DUST; LOTUS; POSS; WETTABILITY; ROUGHNESS; BEHAVIOR; LEAVES AB Topographically rich surfaces were generated by spray-coating organic solutions of a polyhedral oligomeric silsesquioxane, octakis(dimethylsilyloxy) silsesquioxane (POSS), on Kapton (R) HN films and exposing them to radio frequency generated oxygen plasma. Changes in both surface chemistry and topography were observed. High-resolution scanning electron microscopy indicated substantial modification of the POSS-coated polyimide surface topographies as a result of oxygen plasma exposure. Water contact angles varied from 104 degrees for unexposed POSS-coated surfaces to similar to 5 degrees for samples exposed for 5 h. Modulation of the dispersive and polar contributions to the surface energy was determined using van Oss Good Chaudhury theory. Changes in surface energy are related to potential adhesive interactions with lunar dust simulant particles. (C) 2009 Elsevier B.V. All rights reserved. C1 [Wohl, Christopher J.; Belcher, Marcus A.; Ghose, Sayata] Natl Inst Aerosp, Hampton, VA 23666 USA. [Connell, John W.] NASA, Langley Res Ctr, Hampton, VA 23681 USA. RP Wohl, CJ (reprint author), Natl Inst Aerosp, 100 Explorat Way, Hampton, VA 23666 USA. EM christopher.j.wohl@nasa.gov FU Oak Ridge Associated Universities NASA Post-doctoral Program; Dust Project under the Exploration Science Mission Directorate (ESMD) FX The authors would like to acknowledge Dr. Joan Hudson and Dr. Ya-Ping Sun at the Clemson University Advanced Materials Research Labs EM Lab for their help with XPS measurements and Dr. Peter Lillehei at NASA Langley Research Center and Dr. Kent Watson at The National Institute of Aerospace for scientific and technical support. The authors also acknowledge funding from the Oak Ridge Associated Universities NASA Post-doctoral Program and the Dust Project under the Exploration Science Mission Directorate (ESMD). NR 61 TC 22 Z9 23 U1 2 U2 33 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 JUN 30 PY 2009 VL 255 IS 18 BP 8135 EP 8144 DI 10.1016/j.apsusc.2009.05.030 PG 10 WC Chemistry, Physical; Materials Science, Coatings & Films; Physics, Applied; Physics, Condensed Matter SC Chemistry; Materials Science; Physics GA 463YG UT WOS:000267469500049 ER PT J AU Signorini, SR McClain, CR AF Signorini, Sergio R. McClain, Charles R. TI Effect of uncertainties in climatologic wind, ocean pCO(2), and gas transfer algorithms on the estimate of global sea-air CO2 flux SO GLOBAL BIOGEOCHEMICAL CYCLES LA English DT Article ID SENSOR MICROWAVE IMAGER; ANTHROPOGENIC CO2; IN-SITU; EXCHANGE; SPEED AB This paper addresses the uncertainties of global sea-air CO2 flux estimated on the basis of the sea-air pCO(2) differences and sea-air CO2 gas transfer rate. Uncertainties in the global sea-air flux estimates are identified from different gas transfer algorithms and monthly wind speeds (NCEP-2 and SSM/I). The net global sea-air flux estimates for the contemporary oceans range from 0.9 +/- 0.5 Pg-C a(-1) to 1.3 +/- 0.8 Pg-C a(-1) for reference year 2000. Including the carbon transferred from rivers in the preindustrial steady oceans, the uptake rates for anthropogenic CO2 range from 1.3 +/- 0.6 Pg-C a(-1) to 1.7 +/- 0.8 Pg-C a(-1). For all three gas exchange parameterizations used, the difference between global fluxes using SSM/I and NCEP-2 winds ranged between 3% and 37%. The subtropical regions are the largest sinks of CO2 (-0.8 Pg-C a(-1)), and the equatorial Pacific is the largest source (0.4 Pg-C a(-1)). The North Pacific (-0.4 Pg-C a(-1)) and the North Atlantic (-0.3 Pg-C a(-1)) are also significant sinks of CO2. All the remaining regions have relatively weak net yearly exchanges of CO2. Recent estimates (Takahashi et al., 2009) of sea-air CO2 flux in the ice-free zone of the Southern Ocean (50 degrees S-62 degrees S) reveal a small mean annual flux (-0.06 Pg-C a(-1)) resulting from the cancellation of the summer uptake CO2 flux with the winter release of CO2 caused by deepwater upwelling. Our study results for the same region range from -0.03 to -0.06 Pg-C a(-1), which are within the uncertainties of the estimates. C1 [Signorini, Sergio R.] Sci Applicat Int Corp, Beltsville, MD 20705 USA. [McClain, Charles R.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Signorini, SR (reprint author), Sci Applicat Int Corp, 4600 Powder Mill Rd,Suite 400, Beltsville, MD 20705 USA. EM sergio.signorini@nasa.gov FU NASA Ocean Biogeochemistry Program FX This research was supported by the NASA Ocean Biogeochemistry Program. Taro Takahashi generously provided the surface ocean and atmospheric pCO2 monthly climatology for reference year 2000, advanced copies of papers, and other related data sets. We are also thankful to Rik Wanninkhof and Colm Sweeney for helpful comments. We are grateful to Frank Wentz and Martin Brewer of Remote Sensing Systems for facilitating the SSM/I data access. NR 30 TC 4 Z9 4 U1 0 U2 3 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0886-6236 EI 1944-9224 J9 GLOBAL BIOGEOCHEM CY JI Glob. Biogeochem. Cycle PD JUN 30 PY 2009 VL 23 AR GB2025 DI 10.1029/2008GB003246 PG 14 WC Environmental Sciences; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Environmental Sciences & Ecology; Geology; Meteorology & Atmospheric Sciences GA 466DZ UT WOS:000267642300001 ER PT J AU Williams, JG Turyshev, SG Boggs, DH AF Williams, James G. Turyshev, Slava G. Boggs, Dale H. TI LUNAR LASER RANGING TESTS OF THE EQUIVALENCE PRINCIPLE WITH THE EARTH AND MOON SO MODERN PHYSICS LETTERS A LA English DT Review DE Lunar laser ranging; equivalence principle; tests of general relativity ID GENERAL-RELATIVITY; DARK-MATTER; MASSIVE BODIES; COSMIC ACCELERATION; GRAVITATIONAL MASS; EOTVOS EXPERIMENTS; TROJAN ASTEROIDS; GRAVITY-FIELD; SOLAR-SYSTEM; PARAMETERS AB A primary objective of the lunar laser ranging (LLR) experiment is to provide precise observations of the lunar orbit that contribute to a wide range of science investigations. In particular, time series of the highly accurate measurements of the distance between the Earth and the Moon provide unique information used to determine whether, in accordance with the equivalence principle (EP), these two celestial bodies are falling toward the Sun at the same rate, despite their different masses, compositions, and gravitational self-energies. Thirty-five years since their initiation, analyses of precision laser ranges to the Moon continue to provide increasingly stringent limits on any violation of the EP. Current LLR solutions give (-1.0 +/- 1.4) x 10(-13) for any possible inequality in the ratios of the gravitational and inertial masses for the Earth and Moon, Delta(M-G/M-I). This result, in combination with laboratory experiments on the weak equivalence principle, yields a strong equivalence principle (SEP) test of Delta(M-G/M-I)(SEP) = (-2.0 +/- 2.0) x 10(-13). Such an accurate result allows other tests of gravitational theories. The result of the SEP test translates into a value for the corresponding SEP violation parameter it of (4.4 +/- 4.5) x 10(-4), where eta = 43 - gamma - 3 and both gamma and beta are parametrized post-Newtonian (PPN) parameters. Using the recent result for the parameter - derived from the radiometric tracking data from the Cassini mission, the PPN parameter beta (quantifying the nonlinearity of gravitational superposition) is determined to be beta - 1 = (1.2 +/- 1.1) x 10(-4). We also present the history of the LLR effort and describe the technique that is being used. Focusing on the tests of the EP, we discuss the existing data, and characterize the modeling and data analysis techniques. The robustness of the LLR solutions is demonstrated with several different approaches that are presented in the text. We emphasize that near-term improvements in the LLR accuracy will further advance the research on relativistic gravity in the solar system and, most notably, will continue to provide highly accurate tests of the EP. C1 [Williams, James G.; Turyshev, Slava G.; Boggs, Dale H.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Williams, JG (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. NR 113 TC 0 Z9 0 U1 0 U2 0 PU WORLD SCIENTIFIC PUBL CO PTE LTD PI SINGAPORE PA 5 TOH TUCK LINK, SINGAPORE 596224, SINGAPORE SN 0217-7323 EI 1793-6632 J9 MOD PHYS LETT A JI Mod. Phys. Lett. A PD JUN 28 PY 2009 VL 24 IS 20 BP 1129 EP 1175 PG 47 WC Physics, Nuclear; Physics, Particles & Fields; Physics, Mathematical SC Physics GA 472IN UT WOS:000268123900001 ER PT J AU Manney, GL Schwartz, MJ Kruger, K Santee, ML Pawson, S Lee, JN Daffer, WH Fuller, RA Livesey, NJ AF Manney, Gloria L. Schwartz, Michael J. Krueger, Kirstin Santee, Michelle L. Pawson, Steven Lee, Jae N. Daffer, William H. Fuller, Ryan A. Livesey, Nathaniel J. TI Aura Microwave Limb Sounder observations of dynamics and transport during the record-breaking 2009 Arctic stratospheric major warming SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article AB A major stratospheric sudden warming (SSW) in January 2009 was the strongest and most prolonged on record. Aura Microwave Limb Sounder (MLS) observations are used to provide an overview of dynamics and transport during the 2009 SSW, and to compare with the intense, long-lasting SSW in January 2006. The Arctic polar vortex split during the 2009 SSW, whereas the 2006 SSW was a vortex displacement event. Winds reversed to easterly more rapidly and reverted to westerly more slowly in 2009 than in 2006. More mixing of trace gases out of the vortex during the decay of the vortex fragments, and less before the fulfillment of major SSW criteria, was seen in 2009 than in 2006; persistent well-defined fragments of vortex and anticyclone air were more prevalent in 2009. The 2009 SSW had a more profound impact on the lower stratosphere than any previously observed SSW, with no significant recovery of the vortex in that region. The stratopause breakdown and subsequent reformation at very high altitude, accompanied by enhanced descent into a rapidly strengthening upper stratospheric vortex, were similar in 2009 and 2006. Many differences between 2006 and 2009 appear to be related to the different character of the SSWs in the two years. Citation: Manney, G. L., M. J. Schwartz, K. Kruger, M. L. Santee, S. Pawson, J. N. Lee, W. H. Daffer, R. A. Fuller, and N. J. Livesey (2009), Aura Microwave Limb Sounder observations of dynamics and transport during the record-breaking 2009 Arctic stratospheric major warming, Geophys. Res. Lett., 36, L12815, doi:10.1029/2009GL038586. C1 [Manney, Gloria L.; Schwartz, Michael J.; Santee, Michelle L.; Lee, Jae N.; Daffer, William H.; Fuller, Ryan A.; Livesey, Nathaniel J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Krueger, Kirstin] Univ Kiel, Leibniz Inst Marine Sci, D-24105 Kiel, Germany. [Pawson, Steven] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Manney, Gloria L.] New Mexico Inst Min & Technol, Socorro, NM 87801 USA. RP Manney, GL (reprint author), CALTECH, Jet Prop Lab, Mail Stop 183-701, Pasadena, CA 91109 USA. EM gloria.l.manney@jpl.nasa.gov RI Schwartz, Michael/F-5172-2016; Pawson, Steven/I-1865-2014 OI Schwartz, Michael/0000-0001-6169-5094; Pawson, Steven/0000-0003-0200-717X FU MLS Team; NASA's GMAO; National Aeronautics and Space Administration FX We thank the MLS Team for their support; NASA's GMAO for the GEOS-5 analyses; and Ken Minschwaner, Dong Wu, Doug Allen, and Michaela Hegglin for helpful discussions. Research at the Jet Propulsion Laboratory, California Institute of Technology, is done under contract with the National Aeronautics and Space Administration. NR 16 TC 197 Z9 200 U1 2 U2 18 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 JUN 27 PY 2009 VL 36 AR L12815 DI 10.1029/2009GL038586 PG 5 WC Geosciences, Multidisciplinary SC Geology GA 464FC UT WOS:000267489700002 ER PT J AU Xiong, XX Wenny, BN Barnes, WL AF Xiong, Xiaoxiong (Jack) Wenny, Brian N. Barnes, William L. TI Overview of NASA Earth Observing Systems Terra and Aqua moderate resolution imaging spectroradiometer instrument calibration algorithms and on-orbit performance SO JOURNAL OF APPLIED REMOTE SENSING LA English DT Article DE MODIS; calibration; radiometric; spectral; spatial; on-board calibrators ID THERMAL EMISSIVE BANDS; REFLECTIVE SOLAR BANDS; MODIS; WATER AB Since launch, the Terra and Aqua moderate resolution imaging spectroradiometer (MODIS) instruments have successfully operated on-orbit for more than 9 and 6.5 years, respectively. MODIS, a key instrument for the NASA's Earth Observing System (EOS) missions, was designed to make continuous observations for studies of Earth's land, ocean, and atmospheric properties and to extend existing data records from heritage earth-observing sensors. In addition to frequent global coverage, MODIS observations are made in 36 spectral bands, covering both solar reflective and thermal emissive spectral regions. Nearly 40 data products are routinely generated from MODIS observations and publicly distributed for a broad range of applications. Both instruments have produced an unprecedented amount of data in support of the science community. As a general reference for understanding sensor operation and calibration, and thus science data quality, we provide an overview of the MODIS instruments and their pre-launch calibration and characterization, and describe their on-orbit calibration algorithms and performance. On-orbit results from both Terra and Aqua MODIS radiometric, spectral, and spatial calibration are discussed. Currently, both instruments, including their on-board calibration devices, are healthy and are expected to continue operation for several years to come. C1 [Xiong, Xiaoxiong (Jack)] NASA, Sci & Explorat Directorate, GSFC, Greenbelt, MD 20771 USA. [Wenny, Brian N.] Sci Syst & Applicat Inc, Lanham, MD 20706 USA. [Barnes, William L.] Univ Maryland Baltimore Cty, Joint Ctr Earth Syst Technol, Catonsville, MD 21228 USA. RP Xiong, XX (reprint author), NASA, Sci & Explorat Directorate, GSFC, Greenbelt, MD 20771 USA. EM Xiaoxiong.Xiong-1@nasa.gov; Brian_Wenny@ssaihq.com; wlbarnes9@gvtc.com NR 35 TC 39 Z9 39 U1 1 U2 6 PU SPIE-SOC PHOTO-OPTICAL INSTRUMENTATION ENGINEERS PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98225 USA SN 1931-3195 J9 J APPL REMOTE SENS JI J. Appl. Remote Sens. PD JUN 26 PY 2009 VL 3 AR 032501 DI 10.1117/1.3180864 PG 25 WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic Technology SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science & Photographic Technology GA 520XB UT WOS:000271881800001 ER PT J AU Burlaga, LF Ness, NF Acuna, MH Wang, YM Sheeley, NR AF Burlaga, L. F. Ness, N. F. Acuna, M. H. Wang, Y. -M. Sheeley, N. R., Jr. TI Radial and solar cycle variations of the magnetic fields in the heliosheath: Voyager 1 observations from 2005 to 2008 SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article ID LOCAL INTERSTELLAR-MEDIUM; WIND TERMINATION SHOCK; ULYSSES OBSERVATIONS; SECTOR STRUCTURE; HELIOSPHERIC ASYMMETRIES; OUTER HELIOSPHERE; FLOW DOWNSTREAM; CURRENT SHEET; INTERPLANETARY; MODEL AB We discuss the magnetic field strength B(t) and polarity observed by Voyager 1 (V1) in the heliosheath at the heliographic latitude approximate to 34 degrees as it moved away from the Sun from 2005 through 2008.82 (where 2008.0 is the beginning of 1 January 2008). The pattern of the polarity of the magnetic field changed from alternating positive and negative polarities to predominantly negative polarities ( magnetic fields pointing along the Archimedean spiral field angle toward the Sun) at approximate to 2006.23). This transition indicates that the latitudinal extent of the heliospheric current sheet (HCS) was decreasing in the supersonic solar wind, as expected for the declining phase of the solar cycle, and as predicted by extrapolation of the magnetic neutral line near the photosphere to the position of V1. However, the polarity was not uniformly negative in during 2008, in contrast to the predicted polarity. This difference suggests that the maximum latitudinal extent of the HCS was tending to increase in the northern hemisphere in the heliosheath, while it was decreasing in the supersonic solar wind. The large-scale magnetic field strength B( t) was observed by V1 from 2005 through 2008.82. During this interval of decreasing solar activity toward solar minimum, B( t) at 1 AU was decreasing, and the solar wind speed V at the latitude of V1 was increasing. Adjusting the temporal profile of B( t) observed by V1 for the solar cycle variations of B and V in the supersonic solar wind, we find that the radial gradient of B( R) in heliosheath from the radial distance R = 94.2 AU to 107.9 AU between 2005.0 and 2008.82 was 0.0017 nT/AU <= grad B <= 0.0055 nT/AU, or grad B = (0.0036 +/- 0.0019) nT/AU. C1 [Burlaga, L. F.] NASA, Goddard Space Flight Ctr, Geospace Phys Lab, Greenbelt, MD 20771 USA. [Acuna, M. H.] NASA, Goddard Space Flight Ctr, Planetary Magnetospheres Lab, Greenbelt, MD 20771 USA. [Ness, N. F.] Catholic Univ Amer, Inst Astrophys & Computat Sci, Washington, DC 20064 USA. [Wang, Y. -M.; Sheeley, N. R., Jr.] USN, Res Lab, EO Hulburt Ctr Space Res, Washington, DC 20375 USA. RP Burlaga, LF (reprint author), NASA, Goddard Space Flight Ctr, Geospace Phys Lab, Mail Code 673,Bldg 21,Room 244, Greenbelt, MD 20771 USA. EM burlaga@lepvax.gsfc; nfness@bartol.udel.edu; mario.h.acuna@nasa.gov; yi.wang@nrl.navy.mil; neil.sheeley@nrl.navy.mil FU NASA [NNX06AG99G] FX T. McClanahan and S. Kramer provided help in the processing of the data. Daniel Berdischevsky computed the zero level offsets for the instrument for the data. N. F. Ness was partially supported in part by NASA grant NNX06AG99G to CUA. One of the authors ( L. B.) acknowledges helpful conversations with N. Pogorelov. NR 52 TC 12 Z9 12 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 JUN 26 PY 2009 VL 114 AR A06106 DI 10.1029/2009JA014071 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 464FY UT WOS:000267491900004 ER PT J AU Schneider, NM Burger, MH Schaller, EL Brown, ME Johnson, RE Kargel, JS Dougherty, MK Achilleos, NA AF Schneider, Nicholas M. Burger, Matthew H. Schaller, Emily L. Brown, Michael E. Johnson, Robert E. Kargel, Jeffrey S. Dougherty, Michele K. Achilleos, Nicholas A. TI No sodium in the vapour plumes of Enceladus SO NATURE LA English DT Article ID DISCOVERY; ATMOSPHERE; SPECTROMETER; ORIGIN AB The discovery of water vapour and ice particles erupting from Saturn's moon Enceladus fuelled speculation that an internal ocean was the source(1-3). Alternatively, the source might be ice warmed, melted or crushed by tectonic motions(4). Sodium chloride (that is, salt) is expected to be present in a long-lived ocean in contact with a rocky core. Here we report a ground-based spectroscopic search for atomic sodium near Enceladus that places an upper limit on the mixing ratio in the vapour plumes orders of magnitude below the expected ocean salinity(5). The low sodium content of escaping vapour, together with the small fraction of salt-bearing particles(6), argues against a situation in which a near-surface geyser is fuelled by a salty ocean through cracks in the crust(1). The lack of observable sodium in the vapour is consistent with a wide variety of alternative eruption sources, including a deep ocean(6), a freshwater reservoir, or ice. The existing data may be insufficient to distinguish between these hypotheses. C1 [Schneider, Nicholas M.] Univ Colorado, Atmospher & Space Phys Lab, Boulder, CO 80309 USA. [Burger, Matthew H.] Univ Maryland Baltimore Cty, Greenbelt, MD 20771 USA. [Burger, Matthew H.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Schaller, Emily L.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. [Brown, Michael E.] CALTECH, Pasadena, CA 91125 USA. [Johnson, Robert E.] Univ Virginia, Charlottesville, VA 22904 USA. [Kargel, Jeffrey S.] Univ Arizona, Tucson, AZ 85721 USA. [Dougherty, Michele K.] Univ London Imperial Coll Sci Technol & Med, London SW7 2AZ, England. [Achilleos, Nicholas A.] UCL, London WC1E 6BT, England. RP Schneider, NM (reprint author), Univ Colorado, Atmospher & Space Phys Lab, Campus Box 392, Boulder, CO 80309 USA. EM nick.schneider@lasp.colorado.edu RI Burger, Matthew/C-1310-2011; OI Achilleos, Nicholas/0000-0002-5886-3509; SCHNEIDER, NICHOLAS/0000-0001-6720-5519 FU W. M. Keck Foundation; National Science Foundation's Planetary Astronomy Program; NASA Postdoctoral Program FX Some of the data presented here were obtained at the W. M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California and the National Aeronautics and Space Administration. The Observatory was made possible by the financial support of the W. M. Keck Foundation. We also acknowledge the Anglo-Australian Telescope and its staff. This work was supported by the National Science Foundation's Planetary Astronomy Program and the NASA Postdoctoral Program. This paper has benefited from discussions with M. Zolotov, J. Spencer, C. Porco, T. Johnson, A. Ingersoll, W. McKinnon, C. Mackay, F. Postberg, J. Schmidt, S. Kempf and R. Pappalardo. NR 23 TC 21 Z9 21 U1 0 U2 12 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 0028-0836 EI 1476-4687 J9 NATURE JI Nature PD JUN 25 PY 2009 VL 459 IS 7250 BP 1102 EP 1104 DI 10.1038/nature08070 PG 3 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 466BX UT WOS:000267636700037 PM 19553993 ER PT J AU MacNeice, P AF MacNeice, Peter TI Validation of community models: Identifying events in space weather model timelines SO SPACE WEATHER-THE INTERNATIONAL JOURNAL OF RESEARCH AND APPLICATIONS LA English DT Article AB I develop and document a set of procedures which test the quality of predictions of solar wind speed and polarity of the interplanetary magnetic field (IMF) made by coupled models of the ambient solar corona and heliosphere. The Wang-Sheeley-Arge (WSA) model is used to illustrate the application of these validation procedures. I present an algorithm which detects transitions of the solar wind from slow to high speed. I also present an algorithm which processes the measured polarity of the outward directed component of the IMF. This removes high-frequency variations to expose the longer-scale changes that reflect IMF sector changes. I apply these algorithms to WSA model predictions made using a small set of photospheric synoptic magnetograms obtained by the Global Oscillation Network Group as input to the model. The results of this preliminary validation of the WSA model (version 1.6) are summarized. C1 NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP MacNeice, P (reprint author), NASA, Goddard Space Flight Ctr, Mail Code 674, Greenbelt, MD 20771 USA. EM peter.j.macNeice@nasa.gov RI MacNeice, Peter/F-5587-2012 FU Community Coordinated Modeling Center FX I would like to acknowledge that without C. N. Arge's extensive support this study would not have been possible. I also wish to acknowledge the support of numerous members of the support staff at the Community Coordinated Modeling Center. The OMNI data were obtained from the GSFC/SPDF Omniweb interface at http://omniweb.gsfc.nasa.gov. I would also like to acknowledge the anonymous referees whose comments helped to improve the papers clarity. NR 11 TC 12 Z9 12 U1 0 U2 2 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 JUN 25 PY 2009 VL 7 AR S06004 DI 10.1029/2009SW000463 PG 10 WC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology & Atmospheric Sciences SC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology & Atmospheric Sciences GA 464GC UT WOS:000267492300002 ER PT J AU Uchida, H Tsunemi, H Katsuda, S Kimura, M Kosugi, H Takahashi, H AF Uchida, Hiroyuki Tsunemi, Hiroshi Katsuda, Satoru Kimura, Masashi Kosugi, Hiroko Takahashi, Hiroaki TI Abundance Inhomogeneity in the Northern Rim of the Cygnus Loop SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN LA English DT Article DE ISM: abundances; ISM: individual (Cygnus Loop); ISM: supernova remnants; X-rays: ISM ID X-RAY-SPECTRUM; HUBBLE-SPACE-TELESCOPE; SUPERNOVA REMNANT; NORTHEASTERN RIM; PLASMA STRUCTURE; SOUTHWESTERN RIM; SUZAKU; EMISSION; ABSORPTION; REGION AB We observed the northern rim of the Cygnus Loop with the Suzaku observatory in 5 pointings (P21-P25). From a spatially resolved analysis, all of the spectra were well fitted by a single component of the non-equilibrium ionization plasma model. From the best-fit parameters, we found that the abundances of the heavy elements are significantly lower than the solar values, except for those at the outermost edge in P21 and P22. The origin of the depleted metal abundances is still unclear, while such deficiencies have been reported from many other rim observations of the Loop. To explain these depletions at the rim regions, we considered several possibilities. The effects of resonance-line-scattering and grain condensation lower the values of the abundances. However, these are not sufficient to account for the observed abundance depletion. We found that the abundances at the outermost edge in P21 and P22 are higher than those at the other regions. From a morphological point of view, it is reasonable to consider that this abundance inhomogeneity is derived from the breakout or the thinness of the cavity wall of the Loop. C1 [Uchida, Hiroyuki; Tsunemi, Hiroshi; Katsuda, Satoru; Kimura, Masashi; Kosugi, Hiroko; Takahashi, Hiroaki] Osaka Univ, Grad Sch Sci, Dept Earth & Space Sci, Osaka 5600043, Japan. [Katsuda, Satoru] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Uchida, H (reprint author), Osaka Univ, Grad Sch Sci, Dept Earth & Space Sci, 1-1 Machikaneyama, Osaka 5600043, Japan. EM uchida@ess.sci.osaka-u.ac.jp RI XRAY, SUZAKU/A-1808-2009 FU Ministry of Education, Culture, Sports, Science and Technology [16002004]; JSPS Research Fellowship for Young Scientists FX This work is partly supported by a Grant-in-Aid for Scientific Research by the Ministry of Education, Culture, Sports, Science and Technology (16002004). This study is also carried out as part of the 21st Century COE Program, "Towards a new basic science: depth and synthesis". H.U. and S.K. are supported by JSPS Research Fellowship for Young Scientists. NR 38 TC 7 Z9 7 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 JUN 25 PY 2009 VL 61 IS 3 BP 503 EP 510 DI 10.1093/pasj/61.3.503 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 475OI UT WOS:000268368900014 ER PT J AU Sugita, S Yamaoka, K Ohno, M Tashiro, MS Nakagawa, YE Urata, Y Pal'shin, V Golenetskii, S Sakamoto, T Cummings, J Krimm, H Stamatikos, M Parsons, A Barthelmy, S Gehrels, N AF Sugita, Satoshi Yamaoka, Kazutaka Ohno, Masanori Tashiro, Makoto S. Nakagawa, Yujin E. Urata, Yuji Pal'shin, Valentin Golenetskii, Sergei Sakamoto, Takanori Cummings, Jay Krimm, Hans Stamatikos, Michael Parsons, Ann Barthelmy, Scott Gehrels, Neil TI Suzaku-WAM, Konus-Wind, and Swift-BAT Observations of Prompt Emission of the High-Redshift GRB 050904 SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN LA English DT Article DE gamma rays: observations; stars: individual (GRB 050904) ID GAMMA-RAY BURST; ALL-SKY MONITOR; PEAK ENERGY; LUMINOSITY RELATION; OPTICAL AFTERGLOW; COSMIC EXPLOSION; GRB-050904; ENERGETICS; SPECTRA; BRIGHT AB We present the results of the high-redshift GRB 050904 at z = 6.295 from joint spectral analysis among Swift-BAT, Konus-Wind, and Suzaku-WAM, covering a wide energy range of 15-5000 keV. The nu F-nu spectrum peak energy, E-peak, was measured at 314(-89)(+173) keV, corresponding to 2291(-634)(+1263) keV in the source frame, and the isotropic equivalent radiated energy, E-iso, was estimated to be 1.04(-0.17)(+0.21) x 10(54)erg. Both are among the highest values that have ever been measured. GRBs with such a high E-iso (similar to 10(54) erg) might be associated with prompt optical emission. The derived spectral and energetic parameters are consistent with the correlation between the rest-frame E-p,E-i and the E-iso (Amati relation), but not with the correlation between the intrinsic peak energy E-p,E-i and the collimation-corrected energy E-gamma (Ghirlanda relation), unless the density of the circumburst environment of this burst is much larger than the nominal value, as suggested by other wavelength observations. We also discuss the possibility that this burst is an outlier in the correlation between E-p,E-i and the peak luminosity L-p (Yonetoku relation). C1 [Sugita, Satoshi; Yamaoka, Kazutaka] Aoyama Gakuin Univ, Dept Math & Phys, Kanagawa 2298558, Japan. [Sugita, Satoshi; Nakagawa, Yujin E.] RIKEN, Inst Phys & Chem Res, Wako, Saitama 3510198, Japan. [Ohno, Masanori] Japan Aerosp Explorat Agcy, Inst Space & Astronaut Sci, Sagamihara, Kanagawa 2298510, Japan. [Tashiro, Makoto S.; Urata, Yuji] Saitama Univ, Dept Phys, Sakura Ku, Saitama 3388570, Japan. [Pal'shin, Valentin; Golenetskii, Sergei] AF Ioffe Phys Tech Inst, Expt Astrophys Lab, St Petersburg 194021, Russia. [Sakamoto, Takanori; Cummings, Jay; Krimm, Hans; Stamatikos, Michael; Parsons, Ann; Barthelmy, Scott; Gehrels, Neil] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Sakamoto, Takanori; Stamatikos, Michael] Oak Ridge Associated Univ, Oak Ridge, TN 37831 USA. [Cummings, Jay] Univ Maryland, Joint Ctr Astrophys, Baltimore, MD 21250 USA. [Krimm, Hans] Univ Space Res Assoc, Columbia, MD 21044 USA. [Urata, Yuji] Acad Sinica, Inst Astron & Astrophys, Taipei 106, Taiwan. RP Sugita, S (reprint author), Aoyama Gakuin Univ, Dept Math & Phys, 5-10-1 Fuchinobe, Kanagawa 2298558, Japan. EM sugita@phys.aoyama.ac.jp RI Barthelmy, Scott/D-2943-2012; Gehrels, Neil/D-2971-2012; Parsons, Ann/I-6604-2012; Tashiro, Makoto/J-4562-2012; Pal'shin, Valentin/F-3973-2014; Golenetskii, Sergey/B-3818-2015; XRAY, SUZAKU/A-1808-2009 FU Ministry of Education, Culture, Sports, Science and Technology (MEXT) [19047001]; Special Postdoctoral Researchers Program in RIKEN; Russian Space Agency contract and RFBR [06-02-16070] FX We thank an anonymous referee for useful cornments and suggestions. This research has been supported in part by a Grant-in-Aid for Scientific Research (19047001 KY) of the Ministry of Education, Culture, Sports, Science and Technology (MEXT). Y.E.N. is supported in part by the Special Postdoctoral Researchers Program in RIKEN. The Konus-Wind experiment is supported by a Russian Space Agency contract and RFBR grant 06-02-16070. NR 54 TC 12 Z9 12 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 JUN 25 PY 2009 VL 61 IS 3 BP 521 EP 527 DI 10.1093/pasj/61.3.521 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 475OI UT WOS:000268368900016 ER PT J AU Plante, I Cucinotta, FA AF Plante, Ianik Cucinotta, Francis A. TI Cross sections for the interactions of 1 eV-100 MeV electrons in liquid water and application to Monte-Carlo simulation of HZE radiation tracks SO NEW JOURNAL OF PHYSICS LA English DT Article ID LOW-ENERGY ELECTRONS; ELASTIC-SCATTERING; SUBEXCITATION ELECTRONS; SECONDARY ELECTRONS; CHARGED-PARTICLES; SPACE EXPLORATION; STRUCTURE CODES; RADIOLYSIS; BREMSSTRAHLUNG; IONIZATION AB High charge (Z) and energy (E) (HZE) nuclei are the main contributors to the uncertainty of radiation risk in space. They ionize a large number of molecules when they interact with matter, initiating a complex succession of events that leads to the radiation track structure. Radiation tracks are often studied by Monte-Carlo simulations that provide detailed information on energy deposition and production of radiolytic species that damage cellular components. These simulations require total and differential elastic and inelastic cross sections. Most ionized electrons have low energy; therefore, most calculations and experiments have been performed on electrons below 1 MeV. Electrons of similar to 1-100 MeV are also produced; they interact with many target molecules when they slow down and determine the radial extension of HZE tracks. Much less work has been done in this energy range. In this paper, a simulation code named RETRACKS uses interaction cross sections (including bremsstrahlung) to calculate the stopping power, range and average energy needed to produce an ion pair (W) for electrons up to 100 MeV. It was also used previously with the RITRACKS program to calculate the radial dose of HZE ions. These cross sections should allow the simulation of higher energy HZE ions, which will help improve our models of space radiation risk. C1 [Plante, Ianik; Cucinotta, Francis A.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. [Plante, Ianik] Univ Space Res Assoc, Div Space Life Sci, Houston, TX 77058 USA. RP Plante, I (reprint author), NASA, Lyndon B Johnson Space Ctr, 2101 NASA Pkwy, Houston, TX 77058 USA. EM ianik.plante-1@nasa.gov; Francis.A.Cucinotta@nasa.gov FU NASA FX This work was supported by NASA Space Radiation Risk Assessment Project. NR 65 TC 36 Z9 36 U1 2 U2 8 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 1367-2630 J9 NEW J PHYS JI New J. Phys. PD JUN 24 PY 2009 VL 11 AR 063047 DI 10.1088/1367-2630/11/6/063047 PG 24 WC Physics, Multidisciplinary SC Physics GA 464RH UT WOS:000267523100004 ER PT J AU Karimabadi, H Sipes, TB Wang, Y Lavraud, B Roberts, A AF Karimabadi, H. Sipes, T. B. Wang, Y. Lavraud, B. Roberts, A. TI A new multivariate time series data analysis technique: Automated detection of flux transfer events using Cluster data SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article ID MAXIMUM-LIKELIHOOD; INCOMPLETE DATA; MAGNETOPAUSE; PLASMA AB A new data mining technique called MineTool-TS is introduced which captures the time-lapse information in multivariate time series data through extraction of global features and metafeatures. This technique is developed into a JAVA-based data mining software which automates all the steps in the model building to make it more accessible to nonexperts. As its first application in space sciences, MineTool-TS is used to develop a model for automated detection of flux transfer events ( FTEs) at Earth's magnetopause in the Cluster spacecraft time series data. The model classifies a given time series into one of three categories of non-FTE, magnetosheath FTE, or magnetospheric FTE. One important feature of MineTool- TS is the ability to explore the importance of each variable or combination of variables as indicators of FTEs. FTEs have traditionally been identified on the basis of their magnetic field signatures, but here we find that some plasma variables can also be effective indicators of FTEs. For example, the perpendicular ion temperature yields a model accuracy of similar to 93%, while a model based solely on the normal magnetic field BN yields an accuracy of similar to 95%. This opens up the possibility of searching for more unusual FTEs that may, for example, have no clear BN signature and create a more comprehensive and less biased list of FTEs for statistical studies. We also find that models using GSM coordinates yield comparable accuracy to those using boundary normal coordinates. This is useful since there are regions where magnetopause models are not accurate. Another surprising result is the finding that the algorithm can largely detect FTEs, and even distinguish between magnetosheath and magnetospheric FTEs, solely on the basis of models built from single parameters, something that experts may not do so straightforwardly on the basis of short time series intervals. The most accurate models use a combination of plasma and magnetic field variables and achieve a very high accuracy of prediction of similar to 99%. We explain the high detection accuracies both in terms of the existence of clear physical signatures of FTEs ( for the majority of cases) and in terms of the capability of the data mining technique to explore the data set in a much more thorough fashion than expert human eyes. A list of 1222 FTEs from Cluster data during years 2001-2003 is provided as auxiliary material. C1 [Karimabadi, H.; Sipes, T. B.] SciberQuest Inc, Del Mar, CA USA. [Karimabadi, H.] Univ Calif San Diego, Dept Elect & Comp Engn, La Jolla, CA 92093 USA. [Wang, Y.; Roberts, A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Lavraud, B.] Univ Toulouse, UPS, Ctr Etud Spatiale Rayonnements, F-31028 Toulouse 4, France. [Lavraud, B.] CNRS, UMR5187, Toulouse, France. RP Karimabadi, H (reprint author), SciberQuest Inc, 2130 Via Mar Valle, Del Mar, CA USA. EM homak@sciberquest.com FU NASA LWS [NNH06CD22C]; NASA SBIR Program contract FX The authors are grateful to the Cluster Ion Spectrometry (CIS) and FluxGate Magnetometer (FGM) instrument teams for the use of the data sets. The research of H. Karimabadi and T. Sipes was supported by a NASA LWS grant NNH06CD22C and a NASA SBIR Program contract. The authors acknowledge useful discussions with David Sibeck and Jan Merka. NR 35 TC 5 Z9 5 U1 0 U2 12 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9380 EI 2169-9402 J9 J GEOPHYS RES-SPACE JI J. Geophys. Res-Space Phys. PD JUN 23 PY 2009 VL 114 AR A06216 DI 10.1029/2009JA014202 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 464FV UT WOS:000267491600003 ER PT J AU Shukla, SP Chandler, MA Jonas, J Sohl, LE Mankoff, K Dowsett, H AF Shukla, Sonali P. Chandler, Mark A. Jonas, Jeff Sohl, Linda E. Mankoff, Ken Dowsett, Harry TI Impact of a permanent El Nino (El Padre) and Indian Ocean Dipole in warm Pliocene climates SO PALEOCEANOGRAPHY LA English DT Article ID NORTH-ATLANTIC OCEAN; WESTERN UNITED-STATES; MIDDLE PLIOCENE; SURFACE TEMPERATURES; EQUATORIAL PACIFIC; SEA; CIRCULATION; ATMOSPHERE; RECONSTRUCTION; ENSO AB Pliocene sea surface temperature data, as well as terrestrial precipitation and temperature proxies, indicate warmer than modern conditions in the eastern equatorial Pacific and imply permanent El Nino-like conditions with impacts similar to those of the 1997/1998 El Nino event. Here we use a general circulation model to examine the global-scale effects that result from imposing warm tropical sea surface temperature (SST) anomalies in both modern and Pliocene simulations. Observed SSTs from the 1997/1998 El Nino event were used for the anomalies and incorporate Pacific warming as well as a prominent Indian Ocean Dipole event. Both the permanent El Nino (also called El Padre) and Indian Ocean Dipole (IOD) conditions are necessary to reproduce temperature and precipitation patterns consistent with the global distribution of Pliocene proxy data. These patterns may result from the poleward propagation of planetary waves from the strong convection centers associated with the El Nino and IOD. C1 [Shukla, Sonali P.] Columbia Univ, Dept Earth & Environm Sci, New York, NY 10025 USA. [Shukla, Sonali P.; Chandler, Mark A.; Jonas, Jeff; Sohl, Linda E.; Mankoff, Ken] NASA, Goddard Inst Space Studies, New York, NY 10025 USA. [Dowsett, Harry] US Geol Survey, Reston, VA 20192 USA. [Chandler, Mark A.; Jonas, Jeff; Sohl, Linda E.; Mankoff, Ken] Columbia Univ, Ctr Climate Syst Res, New York, NY 10025 USA. RP Shukla, SP (reprint author), Columbia Univ, Dept Earth & Environm Sci, New York, NY 10025 USA. EM sps2113@columbia.edu FU National Science Foundation [ATM-0323516]; United States Geological Survey; NASA FX Funding for this research was provided by the National Science Foundation, ATM-0323516 (to M. A. C.), the United States Geological Survey, and the NASA Climate Program. Thanks to Christina Ravelo and an anonymous reviewer for comments that helped improve the paper. NR 60 TC 18 Z9 18 U1 0 U2 7 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0883-8305 EI 1944-9186 J9 PALEOCEANOGRAPHY JI Paleoceanography PD JUN 23 PY 2009 VL 24 AR PA2221 DI 10.1029/2008PA001682 PG 12 WC Geosciences, Multidisciplinary; Oceanography; Paleontology SC Geology; Oceanography; Paleontology GA 464GA UT WOS:000267492100002 ER PT J AU Toma, K Sakamoto, T Zhang, B Hill, JE McConnell, ML Bloser, PF Yamazaki, R Ioka, K Nakamura, T AF Toma, Kenji Sakamoto, Takanori Zhang, Bing Hill, Joanne E. McConnell, Mark L. Bloser, Peter F. Yamazaki, Ryo Ioka, Kunihito Nakamura, Takashi TI STATISTICAL PROPERTIES OF GAMMA-RAY BURST POLARIZATION SO ASTROPHYSICAL JOURNAL LA English DT Article DE gamma rays: bursts; magnetic fields; polarization; radiation mechanisms: non-thermal ID MAGNETIC-FIELD STRUCTURE; LIGHT CURVES; POLARIMETER EXPERIMENT; LINEAR-POLARIZATION; GRB 041219A; EMISSION; AFTERGLOW; GRB-030329; SCATTERING; SPECTRA AB The emission mechanism and the origin and structure of magnetic fields in gamma-ray burst (GRB) jets are among the most important open questions concerning the nature of the central engine of GRBs. In spite of extensive observational efforts, these questions remain to be answered and are difficult or even impossible to infer with the spectral and light-curve information currently collected. Polarization measurements will lead to unambiguous answers to several of these questions. Recent developments in X-ray and gamma-ray polarimetry techniques have demonstrated a significant increase in sensitivity, enabling several new mission concepts, e. g., Polarimeters for Energetic Transients (POET), providing wide field of view and broadband polarimetry measurements. If launched, missions of this kind would finally provide definitive measurements of GRB polarizations. We perform Monte Carlo simulations to derive the distribution of GRB polarizations in three emission models; the synchrotron model with a globally ordered magnetic field (SO model), the synchrotron model with a small-scale random magnetic field (SR model), and the Compton drag model (CD model). The results show that POET, or other polarimeters with similar capabilities, can constrain the GRB emission models by using the statistical properties of GRB polarizations. In particular, the ratio of the number of GRBs for which the polarization degrees can be measured to the number of GRBs that are detected (N(m)/N(d)) and the distributions of the polarization degrees (Pi) can be used as the criteria. If N(m)/N(d) > 30% and Pi is clustered between 0.2 and 0.7, the SO model will be favored. If, instead, N(m)/N(d) < 15%, then the SR or CD model will be favored. If several events with Pi > 0.8 are observed, then the CD model will be favored. C1 [Toma, Kenji] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Toma, Kenji] Natl Inst Nat Sci, Natl Astron Observ Japan, Div Theoret Astron, Mitaka, Tokyo 1818588, Japan. [Sakamoto, Takanori; Hill, Joanne E.] CRESST, Greenbelt, MD 20771 USA. [Sakamoto, Takanori; Hill, Joanne E.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Sakamoto, Takanori] Univ Maryland, Joint Ctr Astrophys, Baltimore, MD 21250 USA. [Zhang, Bing] Univ Nevada, Dept Phys & Astron, Las Vegas, NV 89154 USA. [Hill, Joanne E.] Univ Space Res Assoc, Columbia, MD 21044 USA. [McConnell, Mark L.; Bloser, Peter F.] Univ New Hampshire, Ctr Space Sci, Durham, NH 03824 USA. [Yamazaki, Ryo] Hiroshima Univ, Dept Phys Sci, Hiroshima 7398526, Japan. [Ioka, Kunihito] High Energy Accelerator Res Org, Div Theory, Tsukuba, Ibaraki 3050801, Japan. [Nakamura, Takashi] Kyoto Univ, Dept Phys, Kyoto 6068502, Japan. RP Toma, K (reprint author), Penn State Univ, Dept Astron & Astrophys, 525 Davey Lab, University Pk, PA 16802 USA. EM toma@astro.psu.edu FU Ministry of Education, Culture, Sports, Science and Technology (MEXT) of Japan [19047004, 18740153, 18740147, 19540283]; NASA [NNG05GB67G, NNX08AE57A, NNX08AL40G] FX This work is supported in part by the grant-in-aid from the Ministry of Education, Culture, Sports, Science and Technology (MEXT) of Japan, No. 19047004 ( R.Y., K. I., and T.N.), No. 18740153 ( R.Y.), No. 18740147 ( K. I.), No. 19540283 ( T.N.), and in part by the Grant-in-Aid for the global COE program The Next Generation of Physics, Spun from Universality and Emergence from the MEXT of Japan. B.Z. acknowledges NASA NNG05GB67G and NNX08AE57A ( Nevada NASA EPSCoR program) and K. T. acknowledges NASA NNX08AL40G for partial supports. NR 74 TC 43 Z9 44 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 JUN 20 PY 2009 VL 698 IS 2 BP 1042 EP 1053 DI 10.1088/0004-637X/698/2/1042 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 455RQ UT WOS:000266782400007 ER PT J AU Plavchan, P Werner, MW Chen, CH Stapelfeldt, KR Su, KYL Stauffer, JR Song, I AF Plavchan, Peter Werner, M. W. Chen, C. H. Stapelfeldt, K. R. Su, K. Y. L. Stauffer, J. R. Song, I. TI NEW DEBRIS DISKS AROUND YOUNG, LOW-MASS STARS DISCOVERED WITH THE SPITZER SPACE TELESCOPE SO ASTROPHYSICAL JOURNAL LA English DT Review DE circumstellar matter; planetary systems: formation ID MAIN-SEQUENCE STARS; TW-HYDRAE ASSOCIATION; SOLAR-TYPE STARS; MULTIBAND IMAGING PHOTOMETER; STELLAR KINEMATIC GROUPS; URSA-MAJOR GROUP; SUN-LIKE STARS; TERRESTRIAL PLANET FORMATION; PICTORIS MOVING GROUP; VEGA-LIKE STARS AB We present 24 mu m and 70 mu m Multiband Imaging Photometer for Spitzer (MIPS) observations of 70 A through M-type dwarfs with estimated ages from 8 Myr to 1.1 Gyr, as part of a Spitzer guaranteed time program, including a re-analysis of some previously published source photometry. Our sample is selected from stars with common youth indicators such as lithium abundance, X-ray activity, chromospheric activity, and rapid rotation. We compare our MIPS observations to empirically derived K(s)-[24] colors as a function of the stellar effective temperature to identify 24 mu m and 70 mu m excesses. We place constraints or upper limits on dust temperatures and fractional infrared luminosities with a simple blackbody dust model. We confirm the previously published 70 mu m excesses for HD 92945, HD 112429, and AU Mic, and provide updated flux density measurements for these sources. We present the discovery of 70 mu m excesses for five stars: HD 7590, HD 10008, HD 59967, HD 73350, and HD 135599. HD 135599 is also a known Spitzer IRS (InfraRed Spectrograph) excess source, and we confirm the excess at 24 mu m. We also present the detection of 24 mu m excesses for 10 stars: HD 10008, GJ 3400A, HD 73350, HD 112429, HD 123998, HD 175742, AT Mic, BO Mic, HD 358623 and Gl 907.1. We find that large 70 mu m excesses are less common around stars with effective temperatures of less than 5000 K (3.7(-1.1)(+7.6)%) than around stars with effective temperatures between 5000 K and 6000 K (21.4(-5.7)(+9.5)%), despite the cooler stars having a younger median age in our sample (12 Myr vs. 340 Myr). We find that the previously reported excess for TWA 13A at 70 mu m is due to a nearby background galaxy, and the previously reported excess for HD 177724 is due to saturation of the near-infrared photometry used to predict the mid-infrared stellar flux contribution. In the Appendix, we present an updated analysis of dust grain removal timescales due to grain-grain collisions and radiation pressure, Poynting-Robertson (P-R) drag, stellar wind drag, and planet-dust dynamical interaction. We find that drag forces can be important for disk dynamics relative to grain-grain collisions for L(IR)/L(*) < 10(-4), and that stellar wind drag is more important than P-R drag for K and M dwarfs, and possibly for young (< 1 Gyr) G dwarfs as well. C1 [Plavchan, Peter] CALTECH, Ctr Infrared Proc & Anal, Pasadena, CA 91125 USA. [Plavchan, Peter; Werner, M. W.; Stapelfeldt, K. R.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Chen, C. H.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Su, K. Y. L.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Stauffer, J. R.] CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA. [Song, I.] Univ Georgia, Dept Phys & Astron, Athens, GA 30602 USA. RP Plavchan, P (reprint author), CALTECH, Ctr Infrared Proc & Anal, MC 100-22,770 S Wilson Ave, Pasadena, CA 91125 USA. EM plavchan@ipac.caltech.edu RI Stapelfeldt, Karl/D-2721-2012; OI Su, Kate/0000-0002-3532-5580 NR 203 TC 98 Z9 98 U1 0 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUN 20 PY 2009 VL 698 IS 2 BP 1068 EP 1094 DI 10.1088/0004-637X/698/2/1068 PG 27 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 455RQ UT WOS:000266782400010 ER PT J AU Maret, S Bergin, EA Neufeld, DA Green, JD Watson, DM Harwit, MO Kristensen, LE Melnick, GJ Sonnentrucker, P Tolls, V Werner, MW Willacy, K Yuan, Y AF Maret, Sebastien Bergin, Edwin A. Neufeld, David A. Green, Joel D. Watson, Dan M. Harwit, Martin O. Kristensen, Lars E. Melnick, Gary J. Sonnentrucker, Paule Tolls, Volker Werner, Michael W. Willacy, Karen Yuan, Yuan TI SPITZER MAPPING OF MOLECULAR HYDROGEN PURE ROTATIONAL LINES IN NGC 1333: A DETAILED STUDY OF FEEDBACK IN STAR FORMATION SO ASTROPHYSICAL JOURNAL LA English DT Article DE astrochemistry; ISM: abundances; ISM: individual (NGC 1333); ISM: molecules; stars: formation ID YOUNG STELLAR OBJECTS; LOW-MASS PROTOSTARS; HH 7-11; SPACE-TELESCOPE; INFRARED SPECTROGRAPH; NGC-1333 IRAS-4; WATER EMISSION; SHOCK-WAVES; BOW SHOCK; OUTFLOW AB We present mid-infrared spectral maps of the NGC 1333 star-forming region, obtained with the infrared spectrometer on board the Spitzer Space Telescope. Eight pure H(2) rotational lines, from S(0) to S(7), are detected and mapped. The H(2) emission appears to be associated with the warm gas shocked by the multiple outflows present in the region. A comparison between the observed intensities and the predictions of detailed shock models indicates that the emission arises in both slow (12-24 km s(-1)) and fast (36-53 km s(-1)) C-type shocks with an initial ortho-to-para ratio (opr) less than or similar to 1. The present H(2) opr exhibits a large degree of spatial variations. In the postshocked gas, it is usually about 2, i.e., close to the equilibrium value (similar to 3). However, around at least two outflows, we observe a region with a much lower (similar to 0.5) opr. This region probably corresponds to gas which has been heated up recently by the passage of a shock front, but whose ortho-to-para has not reached equilibrium yet. This, together with the low initial opr needed to reproduce the observed emission, provide strong evidence that H(2) is mostly in para form in cold molecular clouds. The H(2) lines are found to contribute to 25%-50% of the total outflow luminosity, and thus can be used to ascertain the importance of star formation feedback on the natal cloud. From these lines, we determine the outflow mass loss rate and, indirectly, the stellar infall rate, the outflow momentum and the kinetic energy injected into the cloud over the embedded phase. The latter is found to exceed the binding energy of individual cores, suggesting that outflows could be the main mechanism for core disruption. C1 [Bergin, Edwin A.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Neufeld, David A.; Sonnentrucker, Paule; Yuan, Yuan] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Green, Joel D.; Watson, Dan M.] Univ Rochester, Dept Phys & Astron, Rochester, NY 14627 USA. Cornell Univ, Dept Astron, Ithaca, NY 14853 USA. [Kristensen, Lars E.] Leiden Observ, NL-2300 RA Leiden, Netherlands. [Melnick, Gary J.; Tolls, Volker] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Werner, Michael W.; Willacy, Karen] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Maret, S (reprint author), Univ Grenoble 1, CNRS, Observ Grenoble, Lab Astrophys Grenoble,UMR 571, BP 53, F-38041 Grenoble, France. RI Kristensen, Lars/F-4774-2011; OI Kristensen, Lars/0000-0003-1159-3721; Maret, Sebastien/0000-0003-1104-4554 FU NASA [20378] FX This work is based on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology under a contract with NASA. Support for this work was provided by NASA through an award issued by JPL/Caltech for program # 20378. Facilities: Spitzer (IRS) NR 70 TC 37 Z9 37 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUN 20 PY 2009 VL 698 IS 2 BP 1244 EP 1260 DI 10.1088/0004-637X/698/2/1244 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 455RQ UT WOS:000266782400023 ER PT J AU Gezari, S Heckman, T Cenko, SB Eracleous, M Forster, K Goncalves, TS Martin, DC Morrissey, P Neff, SG Seibert, M Schiminovich, D Wyder, TK AF Gezari, Suvi Heckman, Tim Cenko, S. Bradley Eracleous, Michael Forster, Karl Goncalves, Thiago S. Martin, D. Chris Morrissey, Patrick Neff, Susan G. Seibert, Mark Schiminovich, David Wyder, Ted K. TI LUMINOUS THERMAL FLARES FROM QUIESCENT SUPERMASSIVE BLACK HOLES SO ASTROPHYSICAL JOURNAL LA English DT Review DE black hole physics; galaxies: nuclei; ultraviolet: ISM; X-rays: galaxies ID ACTIVE GALACTIC NUCLEI; TIDAL DISRUPTION EVENTS; HUBBLE-SPACE-TELESCOPE; HARD X-RAY; STAR-FORMING GALAXIES; DIGITAL SKY SURVEY; BL-LAC OBJECTS; OPTICAL VARIABILITY; STELLAR DISRUPTION; NEARBY GALAXIES AB A dormant supermassive black hole lurking in the center of a galaxy will be revealed when a star passes close enough to be torn apart by tidal forces, and a flare of electromagnetic radiation is emitted when the bound fraction of the stellar debris falls back onto the black hole and is accreted. Although the tidal disruption of a star is a rare event in a galaxy, approximate to 10(-4) yr(-1), observational candidates have emerged in all-sky X-ray and deep ultraviolet (UV) surveys in the form of luminous UV/X-ray flares from otherwise quiescent galaxies. Here we present the third candidate tidal disruption event discovered in the Galaxy Evolution Explorer (GALEX) Deep Imaging Survey: a 1.6 x 10(43) erg s(-1) UV/optical flare from a star-forming galaxy at z = 0.1855. The UV/optical spectral energy distribution (SED) during the peak of the flare measured by GALEX and Palomar Large Field Camera imaging can be modeled as a single temperature blackbody with T-bb = 1.7 x 10(5) K and a bolometric luminosity of 3 x 10(45) erg s(-1), assuming an internal extinction with E(B-V)(gas) = 0.3. The Chandra upper limit on the X-ray luminosity during the peak of the flare, L-X(2-10 keV)< 10(41) erg s(-1), is 2 orders of magnitude fainter than expected from the ratios of UV to X-ray flux density observed in active galaxies. We compare the light curves and broadband properties of all three tidal disruption candidates discovered by GALEX, and find that (1) the light curves are well fitted by the power-law decline expected for the fallback of debris from a tidally disrupted solar-type star and (2) the UV/optical SEDs can be attributed to thermal emission from an envelope of debris located at roughly 10 times the tidal disruption radius of a approximate to 10(7)M(circle dot) central black hole. We use the observed peak absolute optical magnitudes of the flares (-17.5 > M-g > 18.9) to predict the detection capabilities of upcoming optical synoptic surveys. C1 [Gezari, Suvi; Heckman, Tim] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Cenko, S. Bradley] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Eracleous, Michael] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16803 USA. [Forster, Karl; Goncalves, Thiago S.; Martin, D. Chris; Morrissey, Patrick; Wyder, Ted K.] CALTECH, Pasadena, CA 91125 USA. [Neff, Susan G.] NASA, Goddard Space Flight Ctr, Astron & Solar Phys Lab, Greenbelt, MD 20771 USA. [Seibert, Mark] Observ Carnegie Inst Washington, Pasadena, CA 90095 USA. [Schiminovich, David] Columbia Univ, Dept Astron, New York, NY 10027 USA. RP Gezari, S (reprint author), Johns Hopkins Univ, Dept Phys & Astron, 3400 N Charles St, Baltimore, MD 21218 USA. EM suvi@pha.jhu.edu FU NASA [HST-HF-01219.01-A, NAS 5-26555, G07-8112X]; W. M. Keck Foundation; NSF [AST-0071048] FX We thank the anonymous referee for their helpful comments. S. G. was supported by NASA through Hubble Fellowship grant HST-HF-01219.01-A awarded by the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., for NASA, under contract NAS 5-26555, and in part by Chandra grant G07-8112X. We gratefully acknowledge NASA's support for construction, operation, and science analysis for the GALEX mission, developed in cooperation with Centre National d'Etudes Spatiales of France and the Korean Ministry of Science and Technology. Some of the data presented were obtained at the W. M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California, and NASA. The Observatory was make possible by the generous financial support of the W. M. Keck Foundation. The analysis pipeline used to reduce the DEIMOS data was developed at UC Berkeley with support from NSF grant AST-0071048. The Hobby-Eberly Telescope (HET) is a joint project of the University of Texas at Austin, the Pennsylvania State University, Stanford University, Ludwig-Maximillians-Universitat Munchen, and Georg-August-Universitat Gottingen. The HET is named in honor of its principal benefactors, William P. Hobby and Robert E. Eberly. The Marcario Low-Resolution Spectrograph is named for Mike Marcario of High Lonesome Optics, who fabricated several optics for the instrument but died before its completion; it is a joint project of the Hobby-Eberly Telescope partnership and the Instituto de Astronomia de la Universidad Nacional Autonoma de Mexico. NR 104 TC 121 Z9 121 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 JUN 20 PY 2009 VL 698 IS 2 BP 1367 EP 1379 DI 10.1088/0004-637X/698/2/1367 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 455RQ UT WOS:000266782400034 ER PT J AU Graham, JF Fruchter, AS Levan, AJ Melandri, A Kewley, LJ Levesque, EM Nysewander, M Tanvir, NR Dahlen, T Bersier, D Wiersema, K Bonfield, DG Martinez-Sansigre, A AF Graham, J. F. Fruchter, A. S. Levan, A. J. Melandri, A. Kewley, L. J. Levesque, E. M. Nysewander, M. Tanvir, N. R. Dahlen, T. Bersier, D. Wiersema, K. Bonfield, D. G. Martinez-Sansigre, A. TI GRB 070714B-DISCOVERY OF THE HIGHEST SPECTROSCOPICALLY CONFIRMED SHORT BURST REDSHIFT SO ASTROPHYSICAL JOURNAL LA English DT Article DE gamma rays: bursts ID GAMMA-RAY BURSTS; LUMINOUS GALAXY CLUSTER; STAR-FORMATION RATES; HUBBLE DEEP FIELD; HOST GALAXY; NEUTRON-STARS; SPACE-TELESCOPE; X-RAY; AFTERGLOW; CONSTRAINTS AB We detect the optical afterglow and host galaxy of GRB 070714B. Our observations of the afterglow show an initial plateau in the light curve for approximately the first 5-25 minutes, and then steepening to a power-law decay with index alpha = 0.86 +/- 0.10 for the period between 1 and 24 hr postburst. This is consistent with the X-ray light curve which shows an initial plateau followed by a similar subsequent decay. At late time, we detect a host galaxy at the location of the optical transient. Gemini Nod & Shuffle spectroscopic observations of the host show a single emission line at 7167 angstrom which, based on a griz JHK photometric redshift, we conclude is the 3727 angstrom [O II] line. We therefore find a redshift of z = 0.923. This redshift, as well as a subsequent probable spectroscopic redshift determination of GRB 070429B at z = 0.904 by two other groups significantly exceeds the previous highest spectroscopically confirmed short burst redshift of z = 0.546 for GRB 051221. This dramatically moves back the time at which we know short bursts were being formed and suggests that the present evidence for an old progenitor population may be observationally biased. C1 [Graham, J. F.] Johns Hopkins Univ, Dept Phys & Astron, Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Levan, A. J.] Univ Warwick, Dept Phys, Coventry CV4 7AL, W Midlands, England. [Melandri, A.; Bersier, D.] Liverpool John Moores Univ, Astrophys Res Inst, Birkenhead CH41 1LD, Merseyside, England. [Kewley, L. J.; Levesque, E. M.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. [Tanvir, N. R.; Wiersema, K.] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England. [Bonfield, D. G.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Martinez-Sansigre, A.] Max Planck Inst Astron, D-69117 Heidelberg, Germany. RP Graham, JF (reprint author), Johns Hopkins Univ, Dept Phys & Astron, Space Telescope Sci Inst, 3700 San Martin Dr, Baltimore, MD 21218 USA. NR 88 TC 39 Z9 39 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUN 20 PY 2009 VL 698 IS 2 BP 1620 EP 1629 DI 10.1088/0004-637X/698/2/1620 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 455RQ UT WOS:000266782400050 ER PT J AU George, JS Lave, KA Wiedenbeck, ME Binns, WR Cummings, AC Davis, AJ de Nolfo, GA Hink, PL Israel, MH Leske, RA Mewaldt, RA Scott, LM Stone, EC von Rosenvinge, TT Yanasak, NE AF George, J. S. Lave, K. A. Wiedenbeck, M. E. Binns, W. R. Cummings, A. C. Davis, A. J. de Nolfo, G. A. Hink, P. L. Israel, M. H. Leske, R. A. Mewaldt, R. A. Scott, L. M. Stone, E. C. von Rosenvinge, T. T. Yanasak, N. E. TI ELEMENTAL COMPOSITION AND ENERGY SPECTRA OF GALACTIC COSMIC RAYS DURING SOLAR CYCLE 23 SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmic rays; Galaxy: abundances; Sun: activity ID ADVANCED COMPOSITION EXPLORER; ISOTOPIC COMPOSITION; CROSS-SECTIONS; CHARGE COMPOSITION; PROPAGATION; MODULATION; NUCLEI; CONSTRAINTS; ORIGIN; LI AB We report improved measurements of elemental abundances and spectra for galactic cosmic-ray (GCR) nuclei obtained by the Cosmic Ray Isotope Spectrometer on board NASA's Advanced Composition Explorer (ACE) spacecraft during the minimum and maximum phases of solar cycle 23. We discuss results for particles with nuclear charge 5 <= Z <= 28 and typical energies between 50 and 500 MeV nucleon(-1). We demonstrate that a detailed "leaky box" Galactic propagation model combined with a spherically symmetric solar modulation model gives a good (but not perfect) fit to the observed spectra by using a solar modulation parameter of phi = 325 MV at solar minimum and phi = 900 MV at solar maximum. Although our results are generally consistent with previous measurements from space-based and balloon-based missions, there are significant differences. The large geometrical acceptance and excellent charge resolution of the instrument result in the most detailed and statistically significant record of GCR composition to date in this energy range. The measurements reported here serve as a high-precision baseline for continued studies of GCR composition, solar modulation over the solar cycle, space radiation hazards, and other applications. C1 [George, J. S.; Cummings, A. C.; Davis, A. J.; Leske, R. A.; Mewaldt, R. A.; Stone, E. C.] CALTECH, Pasadena, CA 91125 USA. [Lave, K. A.; Binns, W. R.; Hink, P. L.; Israel, M. H.; Scott, L. M.] Washington Univ, Dept Phys, St Louis, MO 63130 USA. [Wiedenbeck, M. E.; Yanasak, N. E.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [de Nolfo, G. A.; von Rosenvinge, T. T.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP George, JS (reprint author), Aerosp Corp, Dept Space Sci, POB 92957, Los Angeles, CA 90009 USA. RI de Nolfo, Georgia/E-1500-2012 NR 43 TC 46 Z9 46 U1 0 U2 8 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JUN 20 PY 2009 VL 698 IS 2 BP 1666 EP 1681 DI 10.1088/0004-637X/698/2/1666 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 455RQ UT WOS:000266782400054 ER PT J AU Heinis, S Budavari, T Szalay, AS Arnouts, S Aragon-Calvo, MA Wyder, TK Barlow, TA Foster, K Peter, FG Martin, DC Morrissey, P Neff, SG Schiminovich, D Seibert, M Bianchi, L Donas, J Heckman, TM Lee, YW Madore, BF Milliard, B Rich, RM Yi, SK AF Heinis, Sebastien Budavari, Tamas Szalay, Alex S. Arnouts, Stephane Aragon-Calvo, Miguel A. Wyder, Ted K. Barlow, Tom A. Foster, Karl Peter, Friedman G. Martin, D. Christopher Morrissey, Patrick Neff, Susan G. Schiminovich, David Seibert, Mark Bianchi, Luciana Donas, Jose Heckman, Timothy M. Lee, Young-Wook Madore, Barry F. Milliard, Bruno Rich, R. Michael Yi, Sukyoung K. TI SPATIAL CLUSTERING FROM GALEX-SDSS SAMPLES: STAR FORMATION HISTORY AND LARGE-SCALE CLUSTERING SO ASTROPHYSICAL JOURNAL LA English DT Article DE ultraviolet: galaxies ID DIGITAL-SKY-SURVEY; GALAXY REDSHIFT SURVEY; HALO OCCUPATION DISTRIBUTION; COLOR-MAGNITUDE DIAGRAM; LYMAN BREAK GALAXIES; VLT DEEP SURVEY; ACTIVE GALACTIC NUCLEI; UV-SELECTED GALAXIES; EARLY DATA RELEASE; STELLAR MASS AB We measure the projected spatial correlation function w(p)(r(p)) from a large sample combining Galaxy Evolution Explorer ultraviolet imaging with the Sloan Digital Sky Survey spectroscopic sample. We study the dependence of the clustering strength for samples selected on (NUV - r)(abs) color, specific star formation rate (SSFR), and stellar mass. We find that there is a smooth transition in the clustering of galaxies as a function of this color from weak clustering among blue galaxies to stronger clustering for red galaxies. The clustering of galaxies within the "green valley" has an intermediate strength, and is consistent with that expected from galaxy groups. The results are robust to the correction for dust extinction. The comparison with simple analytical modeling suggests that the halo occupation number increases with older star formation epochs. When splitting according to SSFR, we find that the SSFR is a more sensitive tracer of environment than stellar mass. C1 [Heinis, Sebastien; Budavari, Tamas; Szalay, Alex S.; Aragon-Calvo, Miguel A.; Bianchi, Luciana; Heckman, Timothy M.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Arnouts, Stephane] Canada France Hawaii Telescope Corp, Kamuela, HI 96743 USA. [Wyder, Ted K.; Barlow, Tom A.; Foster, Karl; Peter, Friedman G.; Martin, D. Christopher; Morrissey, Patrick] CALTECH, Pasadena, CA 91125 USA. [Neff, Susan G.] NASA, Goddard Space Flight Ctr, Astron & Solar Phys Lab, Greenbelt, MD 20771 USA. [Schiminovich, David] Columbia Univ, Dept Astron, New York, NY 10027 USA. [Seibert, Mark; Madore, Barry F.] Observ Carnegie Inst Washington, Pasadena, CA 91101 USA. [Donas, Jose; Milliard, Bruno] CNRS, Astrophys Lab, F-13388 Marseille 13, France. [Lee, Young-Wook; Yi, Sukyoung K.] Yonsei Univ, Ctr Space Astrophys, Seoul 120749, South Korea. [Rich, R. Michael] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA. RP Heinis, S (reprint author), Johns Hopkins Univ, Dept Phys & Astron, Homewood Campus, Baltimore, MD 21218 USA. NR 92 TC 13 Z9 13 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUN 20 PY 2009 VL 698 IS 2 BP 1838 EP 1851 DI 10.1088/0004-637X/698/2/1838 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 455RQ UT WOS:000266782400068 ER PT J AU Muzzin, A Wilson, G Yee, HKC Hoekstra, H Gilbank, D Surace, J Lacy, M Blindert, K Majumdar, S Demarco, R Gardner, JP Gladders, M Lonsdale, C AF Muzzin, Adam Wilson, Gillian Yee, H. K. C. Hoekstra, Henk Gilbank, David Surace, Jason Lacy, Mark Blindert, Kris Majumdar, Subhabrata Demarco, Ricardo Gardner, Jonathan P. Gladders, Mike Lonsdale, Carol TI SPECTROSCOPIC CONFIRMATION OF TWO MASSIVE RED-SEQUENCE-SELECTED GALAXY CLUSTERS AT z similar to 1.2 IN THE SpARCS-NORTH CLUSTER SURVEY SO ASTROPHYSICAL JOURNAL LA English DT Article DE infrared: galaxies ID MORPHOLOGY-DENSITY RELATION; DIGITAL SKY SURVEY; HIGH-REDSHIFT CLUSTERS; IRAC SHALLOW SURVEY; STAR-FORMATION; X-RAY; ENVIRONMENTAL DEPENDENCE; Z-SIMILAR-TO-1 CLUSTERS; VELOCITY DISPERSIONS; LUMINOSITY FUNCTIONS AB The Spitzer Adaptation of the Red-sequence Cluster Survey (SpARCS) is a deep z'-band imaging survey covering the Spitzer Wide-Area Infrared Extragalactic Survey (SWIRE) Legacy fields designed to create the first large homogeneously selected sample of massive clusters at z > 1 using an infrared adaptation of the cluster red-sequence method. We present an overview of the northern component of the survey which has been observed with Canada-France-Hawaii Telescope (CFHT)/MegaCam and covers 28.3 deg(2). The southern component of the survey was observed with Cerro Tololo Inter-American Observatory (CTIO)/MOSAICII, covers 13.6 deg(2), and is summarized in a companion paper by Wilson et al. We also present spectroscopic confirmation of two rich cluster candidates at z similar to 1.2. Based on Nod-and-Shuffle spectroscopy from GMOS-N on Gemini, there are 17 and 28 confirmed cluster members in SpARCS J163435+402151 and SpARCS J163852+403843 which have spectroscopic redshifts of 1.1798 and 1.1963, respectively. The clusters have velocity dispersions of 490 +/- 140 km s(-1) and 650 +/- 160 km s(-1), respectively, which imply masses (M(200)) of (1.0 +/- 0.9) x 10(14) M(circle dot). Conformation of these candidates as bona fide massive clusters demonstrates that two-filter imaging is an effective, yet observationally efficient, method for selecting clusters at z > 1. C1 [Muzzin, Adam] Yale Univ, Dept Astron, New Haven, CT 06520 USA. [Wilson, Gillian; Demarco, Ricardo] Univ Calif Riverside, Dept Phys & Astron, Riverside, CA 92521 USA. [Yee, H. K. C.] Univ Toronto, Dept Astron & Astrophys, Toronto, ON M5S 3H4, Canada. [Hoekstra, Henk] Univ Victoria, Dept Phys & Astron, Victoria, BC V8P 5C2, Canada. [Hoekstra, Henk] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. [Gilbank, David] Univ Waterloo, Dept Phys & Astron, Astrophys & Gravitat Grp, Waterloo, ON N2L 3G1, Canada. [Surace, Jason; Lacy, Mark] CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA. [Blindert, Kris] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Majumdar, Subhabrata] Tata Inst Fundamental Res, Dept Astron & Astrophys, Bombay 400005, Maharashtra, India. [Gardner, Jonathan P.] NASA, Goddard Space Flight Ctr, Lab Observ Cosmol, Greenbelt, MD 20771 USA. [Gladders, Mike] Univ Chicago, Chicago, IL 60637 USA. [Lonsdale, Carol] NRAO Headquarters, N Amer ALMA Sci Ctr, Charlottesville, VA 22903 USA. RP Muzzin, A (reprint author), Yale Univ, Dept Astron, New Haven, CT 06520 USA. EM adam.muzzin@yale.edu OI Hoekstra, Henk/0000-0002-0641-3231 FU NASA FX This work is based in part on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology under a contract with NASA. NR 56 TC 55 Z9 55 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUN 20 PY 2009 VL 698 IS 2 BP 1934 EP 1942 DI 10.1088/0004-637X/698/2/1934 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 455RQ UT WOS:000266782400077 ER PT J AU Wilson, G Muzzin, A Yee, HKC Lacy, M Surace, J Gilbank, D Blindert, K Hoekstra, H Majumdar, S Demarco, R Gardner, JP Gladders, MD Lonsdale, C AF Wilson, Gillian Muzzin, Adam Yee, H. K. C. Lacy, Mark Surace, Jason Gilbank, David Blindert, Kris Hoekstra, Henk Majumdar, Subhabrata Demarco, Ricardo Gardner, Jonathan P. Gladders, Michael D. Lonsdale, Carol TI SPECTROSCOPIC CONFIRMATION OF A MASSIVE RED-SEQUENCE-SELECTED GALAXY CLUSTER AT z=1.34 IN THE SpARCS-SOUTH CLUSTER SURVEY SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmology: observations; galaxies: clusters: general; galaxies: high-redshift; infrared: galaxies surveys ID COLOR-MAGNITUDE RELATION; SPITZER-SPACE-TELESCOPE; IRAC SHALLOW SURVEY; ARRAY CAMERA IRAC; HIGH-REDSHIFT; POPULATION SYNTHESIS; SKY SURVEY; EVOLUTION; CATALOG; DEEP AB The Spitzer Adaptation of the Red-sequence Cluster Survey (SpARCS) is a z'-passband imaging survey, consisting of deep (z' similar or equal to 24 AB) observations made from both hemispheres using the CFHT 3.6 m and CTIO 4 m telescopes. The survey was designed with the primary aim of detecting galaxy clusters at z > 1. In tandem with pre-existing 3.6 mu m observations from the Spitzer Space Telescope SWIRE Legacy Survey, SpARCS detects clusters using an infrared adaptation of the two-filter red-sequence cluster technique. The total effective area of the SpARCS cluster survey is 41.9 deg(2). In this paper, we provide an overview of the 13.6 deg(2) Southern CTIO/MOSAIC II observations. The 28.3 deg(2) Northern CFHT/MegaCam observations are summarized in a companion paper by Muzzin et al. In this paper, we also report spectroscopic confirmation of SpARCS J003550-431224, a very rich galaxy cluster at z = 1.335, discovered in the ELAIS-S1 field. To date, this is the highest spectroscopically confirmed redshift for a galaxy cluster discovered using the red-sequence technique. Based on nine confirmed members, SpARCS J003550-431224 has a preliminary velocity dispersion of 1050 +/- 230 km s(-1). With its proven capability for efficient cluster detection, SpARCS is a demonstration that we have entered an era of large, homogeneously selected z > 1 cluster surveys. C1 [Wilson, Gillian; Demarco, Ricardo] Univ Calif Riverside, Dept Phys & Astron, Riverside, CA 92521 USA. [Muzzin, Adam] Yale Univ, Dept Astron, New Haven, CT 06520 USA. [Yee, H. K. C.] Univ Toronto, Dept Astron & Astrophys, Toronto, ON M5S 3H4, Canada. [Lacy, Mark; Surace, Jason] CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA. [Gilbank, David] Univ Waterloo, Dept Phys & Astron, Astrophys & Gravitat Grp, Waterloo, ON N2L 3G1, Canada. [Blindert, Kris] Max Planck Inst Astron Koenigstuhl, D-69117 Heidelberg, Germany. [Hoekstra, Henk] Univ Victoria, Dept Phys & Astron, Victoria, BC V8P 5C2, Canada. [Hoekstra, Henk] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. [Majumdar, Subhabrata] Tata Inst Fundamental Res, Dept Astron & Astrophys, Bombay 400005, Maharashtra, India. [Gardner, Jonathan P.] NASA, Goddard Space Flight Ctr, Lab Observat Cosmol, Greenbelt, MD 20771 USA. [Gladders, Michael D.] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA. [Lonsdale, Carol] NRAO Headquarters, N Amer ALMA Sci Ctr, Charlottesville, VA 22903 USA. [Lonsdale, Carol] CALTECH, Infrared Proc & Anal Ctr, Pasadena, CA 91125 USA. RP Wilson, G (reprint author), Univ Calif Riverside, Dept Phys & Astron, Riverside, CA 92521 USA. EM gillianw@ucr.edu OI Hoekstra, Henk/0000-0002-0641-3231 FU JPL/Caltech; College of Natural and Agricultural Sciences FX This work is based in part on archival data obtained with Spitzer, which is operated by the Jet Propulsion Laboratory, California Institute of Technology under a contract with NASA. Support for this work was provided by an award issued by JPL/Caltech. G. W. acknowledges support from the College of Natural and Agricultural Sciences at UCR. NR 51 TC 65 Z9 65 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUN 20 PY 2009 VL 698 IS 2 BP 1943 EP 1950 DI 10.1088/0004-637X/698/2/1943 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 455RQ UT WOS:000266782400078 ER PT J AU Yu, SS Drouin, BJ Pearson, JC Pickett, HM Lattanzi, V Walters, A AF Yu, Shanshan Drouin, Brian J. Pearson, John C. Pickett, Herbert M. Lattanzi, Valerio Walters, Adam TI TERAHERTZ SPECTROSCOPY AND GLOBAL ANALYSIS OF THE BENDING VIBRATIONS OF ACETYLENE (C2D2)-C-12 SO ASTROPHYSICAL JOURNAL LA English DT Article DE catalogs; ISM: molecules; methods: laboratory; molecular data; techniques: spectroscopic ID GRAIN SURFACE-CHEMISTRY; TRIPLY DEUTERATED AMMONIA; DENSE INTERSTELLAR CORES; CM(-1) SPECTRAL REGION; ABSORPTION-SPECTRUM; IRAS 16293-2422; 1ST DETECTION; MOLECULES; D2CO; FORMALDEHYDE AB Two hundred and fifty-one (C2D2)-C-12 transitions have been measured in the 0.2-1.6 THz region of its nu(5)-nu(4) difference band and 202 of them were observed for the first time. The accuracy of these measurements is estimated to be ranging from 50 kHz to 100 kHz. The (C2D2)-C-12 molecules were generated under room temperature by passing 120-150 mTorr D2O vapor through calcium carbide (CaC2) powder. A multistate analysis was carried out for the bending vibrational modes nu(4) and nu(5) of (C2D2)-C-12, which includes the lines observed in this work and prior microwave, far-infrared and infrared data on the pure bending levels. Significantly improved molecular parameters were obtained for (C2D2)-C-12 by adding the new measurements to the old data set, which had only 10 lines with microwave measurement precision. New frequency and intensity predictions have been made based on the obtained molecular parameters. The more precise measurements and new predictions reported here will support the analyses of astronomical observations by the future high-resolution spectroscopy telescopes such as Herschel, SOFIA, and ALMA, which will work in the terahertz spectral region. C1 [Yu, Shanshan; Drouin, Brian J.; Pearson, John C.; Pickett, Herbert M.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Lattanzi, Valerio; Walters, Adam] Univ Toulouse UPS, Ctr Etud Spatiale Rayonnements, CNRS UMR 5187, F-31028 Toulouse 4, France. RP Yu, SS (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM shanshan.yu@jpl.nasa.gov RI Yu, Shanshan/D-8733-2016 FU NASA FX The research described in this paper was performed at the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. S.Y. is a NASA Postdoctoral fellow and her research was supported by an appointment to the NASA Postdoctoral Program at the Jet Propulsion Laboratory, administrated by Oak Ridge Associated Universities through a contract with NASA. NR 53 TC 5 Z9 5 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUN 20 PY 2009 VL 698 IS 2 BP 2114 EP 2120 DI 10.1088/0004-637X/698/2/2114 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 455RQ UT WOS:000266782400092 ER PT J AU Abdo, AA Allen, BT Aune, T Berley, D Casanova, S Chen, C Dingus, BL Ellsworth, RW Fleysher, L Fleysher, R Gonzalez, MM Goodman, JA Hoffman, CM Hopper, B Huntemeyer, PH Kolterman, BE Lansdell, CP Linnemann, JT McEnery, JE Mincer, AI Nemethy, P Noyes, D Pretz, J Ryan, JM Parkinson, PMS Shoup, A Sinnis, G Smith, AJ Sullivan, GW Vasileiou, V Walker, GP Williams, DA Yodh, GB AF Abdo, A. A. Allen, B. T. Aune, T. Berley, D. Casanova, S. Chen, C. Dingus, B. L. Ellsworth, R. W. Fleysher, L. Fleysher, R. Gonzalez, M. M. Goodman, J. A. Hoffman, C. M. Hopper, B. Huentemeyer, P. H. Kolterman, B. E. Lansdell, C. P. Linnemann, J. T. McEnery, J. E. Mincer, A. I. Nemethy, P. Noyes, D. Pretz, J. Ryan, J. M. Parkinson, P. M. Saz Shoup, A. Sinnis, G. Smith, A. J. Sullivan, G. W. Vasileiou, V. Walker, G. P. Williams, D. A. Yodh, G. B. TI THE LARGE-SCALE COSMIC-RAY ANISOTROPY AS OBSERVED WITH MILAGRO SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmic rays; Galaxy: halo; ISM: magnetic fields; solar neighborhood; Sun: activity; supernova remnants ID GALACTIC PLANE; INTENSITY AB Results are presented of a harmonic analysis of the large-scale cosmic-ray (CR) anisotropy as observed by the Milagro observatory. We show a two-dimensional display of the sidereal anisotropy projections in right ascension (R.A.) generated by the fitting of three harmonics to 18 separate declination bands. The Milagro observatory is a water Cherenkov detector located in the Jemez mountains near Los Alamos, New Mexico. With a high duty cycle and large field of view, Milagro is an excellent instrument for measuring this anisotropy with high sensitivity at TeV energies. The analysis is conducted using a seven-year data sample consisting of more than 95 billion events, the largest such data set in existence. We observe an anisotropy with a magnitude around 0.1% for CRs with a median energy of 6 TeV. The dominant feature is a deficit region of depth (2.49 +/- 0.02 stat. +/- 0.09 sys.) x 10(-3) in the direction of the Galactic north pole centered at 189 deg R.A. We observe a steady increase in the magnitude of the signal over seven years. C1 [Abdo, A. A.] Natl Acad Sci, Natl Res Council Res Associate, Washington, DC 20001 USA. [Abdo, A. A.] USN, Res Lab, Div Space Sci, Washington, DC 20375 USA. [Allen, B. T.; Chen, C.; Yodh, G. B.] Univ Calif Irvine, Dept Phys & Astron, Irvine, CA 92697 USA. [Aune, T.; Parkinson, P. M. Saz; Williams, D. A.] Univ Calif Santa Cruz, Santa Cruz Inst Particle Phys, Santa Cruz, CA 95064 USA. [Berley, D.; Goodman, J. A.; Hopper, B.; Lansdell, C. P.; Noyes, D.; Smith, A. J.; Sullivan, G. W.; Vasileiou, V.] Univ Maryland, Dept Phys, College Pk, MD 20742 USA. [Casanova, S.; Dingus, B. L.; Hoffman, C. M.; Huentemeyer, P. H.; Pretz, J.; Sinnis, G.; Walker, G. P.] Los Alamos Natl Lab, Grp P 23, Los Alamos, NM 87545 USA. [Ellsworth, R. W.] George Mason Univ, Dept Phys & Astron, Fairfax, VA 22030 USA. [Fleysher, L.; Fleysher, R.; Kolterman, B. E.; Mincer, A. I.; Nemethy, P.] NYU, Dept Phys, New York, NY 10003 USA. [Gonzalez, M. M.] Univ Nacl Autonoma Mexico, Inst Astron, Mexico City 04510, DF, Mexico. [Linnemann, J. T.] Michigan State Univ, Dept Phys & Astron, E Lansing, MI 48824 USA. [McEnery, J. E.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Ryan, J. M.] Univ New Hampshire, Dept Phys, Durham, NH 03824 USA. [Shoup, A.] Ohio State Univ, Lima, OH 45804 USA. RP Abdo, AA (reprint author), Natl Acad Sci, Natl Res Council Res Associate, Washington, DC 20001 USA. RI McEnery, Julie/D-6612-2012; Casanova, Sabrina/J-8935-2013; OI Casanova, Sabrina/0000-0002-6144-9122; Mincer, Allen/0000-0002-6307-1418 FU National Science Foundation [PHY-0245234, PHY-0302000, PHY-0400424, PHY-0504201, PHY-0601080, ATM-0002744]; US Department of Energy; Los Alamos National Laboratory; University of California; Institute of Geophysics and Planetary Physics FX We acknowledge Scott Delay and Michael Schneider for their dedicated efforts in the construction and maintenance of the Milagro experiment. This work has been supported by the National Science Foundation (under grants PHY-0245234, -0302000, -0400424, -0504201, -0601080, and ATM-0002744) the US Department of Energy (Office of High-Energy Physics and Office of Nuclear Physics), Los Alamos National Laboratory, the University of California, and the Institute of Geophysics and Planetary Physics. NR 22 TC 108 Z9 109 U1 0 U2 9 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUN 20 PY 2009 VL 698 IS 2 BP 2121 EP 2130 DI 10.1088/0004-637X/698/2/2121 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 455RQ UT WOS:000266782400093 ER PT J AU Dennis, BR Pernak, RL AF Dennis, Brian R. Pernak, Rick L. TI HARD X-RAY FLARE SOURCE SIZES MEASURED WITH THE RAMATY HIGH ENERGY SOLAR SPECTROSCOPIC IMAGER SO ASTROPHYSICAL JOURNAL LA English DT Article DE Sun: flares; Sun: X-rays, gamma rays; techniques: image processing ID WHITE-LIGHT; CHROMOSPHERIC EVAPORATION; RHESSI; EMISSION; LOOP; RECONSTRUCTION; TELESCOPE AB Ramaty High Energy Solar Spectroscopic Imager (RHESSI) observations of 18 double hard X-ray sources seen at energies above 25 keV are analyzed to determine the spatial extent of the most compact structures evident in each case. The following four image reconstruction algorithms were used: Clean, Pixon, and two routines using visibilities-maximum entropy and forward fit (VFF). All have been adapted for this study to optimize their ability to provide reliable estimates of the sizes of the more compact sources. The source fluxes, sizes, and morphologies obtained with each method are cross-correlated and the similarities and disagreements are discussed. The full width at half-maximum (FWHM) of the major axes of the sources with assumed elliptical Gaussian shapes are generally well correlated between the four image reconstruction routines and vary between the RHESSI resolution limit of similar to 2 '' up to similar to 20 '' with most below 10 ''. The FWHM of the minor axes are generally at or just above the RHESSI limit and hence should be considered as unresolved in most cases. The orientation angles of the elliptical sources are also well correlated. These results suggest that the elongated sources are generally aligned along a flare ribbon with the minor axis perpendicular to the ribbon. This is verified for the one flare in our list with coincident Transition Region and Coronal Explorer (TRACE) images. There is evidence for significant extra flux in many of the flares in addition to the two identified compact sources, thus rendering the VFF assumption of just two Gaussians inadequate. A more realistic approximation in many cases would be of two line sources with unresolved widths. Recommendations are given for optimizing the RHESSI imaging reconstruction process to ensure that the finest possible details of the source morphology become evident and that reliable estimates can be made of the source dimensions. C1 [Dennis, Brian R.; Pernak, Rick L.] NASA, Goddard Space Flight Ctr, Solar Phys Lab, Heliophys Sci Div, Greenbelt, MD 20771 USA. [Pernak, Rick L.] Catholic Univ Amer, Washington, DC 20064 USA. RP Dennis, BR (reprint author), NASA, Goddard Space Flight Ctr, Solar Phys Lab, Heliophys Sci Div, Code 671, Greenbelt, MD 20771 USA. RI Dennis, Brian/C-9511-2012 FU NASA [NNG06GB96A]; Catholic University of America FX We are grateful to Gordon Hurford and Ed Schmahl for their comments on this paper and help with understanding the RHESSI imaging technique and the different image reconstruction algorithms. We also acknowledge the critical support provided by Kim Tolbert and Richard Schwartz and their help with IDL in general and the SSW procedures in particular. We are grateful to Fred Bruhweiler for managing the NASA Grant NNG06GB96A at The Catholic University of America, through which one of us (R. L. P.) was funded. We acknowledge the contributions of the anonymous referee, who provided many useful comments and corrections that allowed us to significantly improve the paper. NR 30 TC 51 Z9 51 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUN 20 PY 2009 VL 698 IS 2 BP 2131 EP 2143 DI 10.1088/0004-637X/698/2/2131 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 455RQ UT WOS:000266782400094 ER PT J AU Acciari, VA Aliu, E Arlen, T Aune, T Bautista, M Beilicke, M Benbow, W Bradbury, SM Buckley, JH Bugaev, V Butt, Y Byrum, K Cannon, A Celik, O Cesarini, A Chow, YC Ciupik, L Cogan, P Colin, P Cui, W Daniel, MK Dickherber, R Duke, C Dwarkadas, VV Ergin, T Fegan, SJ Finley, JP Finnegan, G Fortin, P Fortson, L Furniss, A Gall, D Gibbs, K Gillanders, GH Godambe, S Grube, J Guenette, R Gyuk, G Hanna, D Hays, E Holder, J Horan, D Hui, CM Humensky, TB Imran, A Kaaret, P Karlsson, N Kertzman, M Kieda, D Kildea, J Konopelko, A Krawczynski, H Krennrich, F Lang, MJ LeBohec, S Maier, G McCann, A McCutcheon, M Millis, J Moriarty, P Ong, RA Otte, AN Pandel, D Perkins, JS Pohl, M Quinn, J Ragan, K Reyes, LC Reynolds, PT Roache, E Rose, HJ Schroedter, M Sembroski, GH Smith, AW Steele, D Swordy, SP Theiling, M Toner, JA Valcarcel, L Varlotta, A Vassiliev, VV Vincent, S Wagner, RG Wakely, SP Ward, JE Weekes, TC Weinstein, A Weisgarber, T Williams, DA Wissel, S Wood, M Zitzer, B AF Acciari, V. A. Aliu, E. Arlen, T. Aune, T. Bautista, M. Beilicke, M. Benbow, W. Bradbury, S. M. Buckley, J. H. Bugaev, V. Butt, Y. Byrum, K. Cannon, A. Celik, O. Cesarini, A. Chow, Y. C. Ciupik, L. Cogan, P. Colin, P. Cui, W. Daniel, M. K. Dickherber, R. Duke, C. Dwarkadas, V. V. Ergin, T. Fegan, S. J. Finley, J. P. Finnegan, G. Fortin, P. Fortson, L. Furniss, A. Gall, D. Gibbs, K. Gillanders, G. H. Godambe, S. Grube, J. Guenette, R. Gyuk, G. Hanna, D. Hays, E. Holder, J. Horan, D. Hui, C. M. Humensky, T. B. Imran, A. Kaaret, P. Karlsson, N. Kertzman, M. Kieda, D. Kildea, J. Konopelko, A. Krawczynski, H. Krennrich, F. Lang, M. J. LeBohec, S. Maier, G. McCann, A. McCutcheon, M. Millis, J. Moriarty, P. Ong, R. A. Otte, A. N. Pandel, D. Perkins, J. S. Pohl, M. Quinn, J. Ragan, K. Reyes, L. C. Reynolds, P. T. Roache, E. Rose, H. J. Schroedter, M. Sembroski, G. H. Smith, A. W. Steele, D. Swordy, S. P. Theiling, M. Toner, J. A. Valcarcel, L. Varlotta, A. Vassiliev, V. V. Vincent, S. Wagner, R. G. Wakely, S. P. Ward, J. E. Weekes, T. C. Weinstein, A. Weisgarber, T. Williams, D. A. Wissel, S. Wood, M. Zitzer, B. TI OBSERVATION OF EXTENDED VERY HIGH ENERGY EMISSION FROM THE SUPERNOVA REMNANT IC 443 WITH VERITAS SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE gamma rays: observations; ISM: individual (IC 443=VER J0616.9+2230, = MAGIC J0616+225) ID GAMMA-RAY EMISSION; XMM-NEWTON OBSERVATIONS; MOLECULAR CLOUDS; MAGIC TELESCOPE; COSMIC-RAYS; IC-443; NEBULA; PULSAR; DISCOVERY; RADIATION AB We present evidence that the very high energy (VHE, E > 100 GeV) gamma-ray emission coincident with the supernova remnant IC 443 is extended. IC 443 contains one of the best studied sites of supernova remnant/molecular cloud interaction and the pulsar wind nebula CXOU J061705.3+222127, both of which are important targets for VHE observations. VERITAS observed IC 443 for 37.9 hr during 2007 and detected emission above 300 GeV with an excess of 247 events, resulting in a significance of 8.3 standard deviations (sigma) before trials and 7.5 sigma after trials in a point-source search. The emission is centered at 6(h)16(m)51(s)+22 degrees 30'11 '' (J2000)+/- 0 degrees.03(stat)+/- 0 degrees.08(sys), with an intrinsic extension of 0 degrees.16 +/- 0 degrees.03(stat)+/- 0 degrees.04(sys). The VHE spectrum is well fit by a power law (dN/dE = N(0) x(E/TeV)(-Gamma)) with a photon index of 2.99 +/- 0.38(stat)+/- 0.3(sys) and an integral flux above 300 GeV of (4.63 +/- 0.90(stat)+/- 0.93(sys)) x 10(-12) cm(-2) s(-1). These results are discussed in the context of existing models for gamma-ray production in IC 443. C1 [Humensky, T. B.; Swordy, S. P.; Wakely, S. P.; Weisgarber, T.; Wissel, S.] Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA. [Acciari, V. A.; Benbow, W.; Gibbs, K.; Kildea, J.; Perkins, J. S.; Roache, E.; Theiling, M.; Weekes, T. C.] Harvard Smithsonian Ctr Astrophys, Fred Lawrence Whipple Observ, Amado, AZ 85645 USA. [Aliu, E.; Holder, J.] Univ Delaware, Dept Phys & Astron, Newark, DE 19716 USA. [Aliu, E.; Holder, J.] Univ Delaware, Bartol Res Inst, Newark, DE 19716 USA. [Arlen, T.; Celik, O.; Chow, Y. C.; Fegan, S. J.; Ong, R. A.; Vassiliev, V. V.; Weinstein, A.; Wood, M.] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA. [Aune, T.; Furniss, A.; Otte, A. N.; Williams, D. A.] Univ Calif Santa Cruz, Santa Cruz Inst Particle Phys, Santa Cruz, CA 95064 USA. [Aune, T.; Furniss, A.; Otte, A. N.; Williams, D. A.] Univ Calif Santa Cruz, Dept Phys, Santa Cruz, CA 95064 USA. [Bautista, M.; Cogan, P.; Guenette, R.; Hanna, D.; Maier, G.; McCann, A.; McCutcheon, M.; Ragan, K.; Valcarcel, L.] McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada. [Beilicke, M.; Buckley, J. H.; Bugaev, V.; Dickherber, R.; Krawczynski, H.] Washington Univ, Dept Phys, St Louis, MO 63130 USA. [Bradbury, S. M.; Daniel, M. K.; Rose, H. J.] Univ Leeds, Sch Phys & Astron, Leeds LS2 9JT, W Yorkshire, England. [Butt, Y.; Ergin, T.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Byrum, K.; Smith, A. W.; Wagner, R. G.] Argonne Natl Lab, Argonne, IL 60439 USA. [Cannon, A.; Grube, J.; Quinn, J.; Ward, J. E.] Univ Coll Dublin, Sch Phys, Dublin 4, Ireland. [Cesarini, A.; Gillanders, G. H.; Lang, M. J.; Toner, J. A.] Natl Univ Ireland, Sch Phys, Galway, Ireland. [Ciupik, L.; Fortson, L.; Gyuk, G.; Karlsson, N.; Steele, D.] Adler Planetarium & Astron Museum, Dept Astron, Chicago, IL 60605 USA. [Colin, P.; Finnegan, G.; Godambe, S.; Hui, C. M.; Kieda, D.; LeBohec, S.; Vincent, S.] Univ Utah, Dept Phys & Astron, Salt Lake City, UT 84112 USA. [Cui, W.; Finley, J. P.; Gall, D.; Sembroski, G. H.; Varlotta, A.; Zitzer, B.] Purdue Univ, Dept Phys, W Lafayette, IN 47907 USA. [Duke, C.] Grinnell Coll, Dept Phys, Grinnell, IA 50112 USA. [Dwarkadas, V. V.] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA. [Fortin, P.] Columbia Univ Barnard Coll, Dept Phys & Astron, New York, NY 10027 USA. [Hays, E.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Horan, D.] Ecole Polytech, CNRS, IN2P3, Lab Leprince Ringuet, F-91128 Palaiseau, France. [Imran, A.; Krennrich, F.; Pohl, M.; Schroedter, M.] Iowa State Univ, Dept Phys & Astron, Ames, IA 50011 USA. [Kaaret, P.; Pandel, D.] Univ Iowa, Dept Phys & Astron, Iowa City, IA 52242 USA. [Kertzman, M.] Depauw Univ, Dept Phys & Astron, Greencastle, IN 46135 USA. [Konopelko, A.] Pittsburg State Univ, Dept Phys, Pittsburg, KS 66762 USA. [Millis, J.] Anderson Univ, Dept Phys, Anderson, IN 46012 USA. [Moriarty, P.] Galway Mayo Inst Technol, Dept Life & Phys Sci, Galway, Ireland. [Reyes, L. C.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA. [Reynolds, P. T.] Cork Inst Technol, Dept Appl Phys & Instrumentat, Cork, Ireland. RP Humensky, TB (reprint author), Univ Chicago, Enrico Fermi Inst, 5640 S Ellis Ave, Chicago, IL 60637 USA. EM humensky@uchicago.edu RI Hays, Elizabeth/D-3257-2012; Daniel, Michael/A-2903-2010; OI Cesarini, Andrea/0000-0002-8611-8610; Cui, Wei/0000-0002-6324-5772; Daniel, Michael/0000-0002-8053-7910; Ward, John E/0000-0003-1973-0794; Otte, Adam Nepomuk/0000-0002-5955-6383; Pandel, Dirk/0000-0003-2085-5586; Lang, Mark/0000-0003-4641-4201 FU US Department of Energy; US National Science Foundation; Smithsonian Institution; NSERC in Canada; Science Foundation Ireland; STFC FX This research is supported by grants from the US Department of Energy, the US National Science Foundation, and the Smithsonian Institution, by NSERC in Canada, by Science Foundation Ireland, and by STFC in the UK. We acknowledge the excellent work of the technical support staff at the FLWO and the collaborating institutions in the construction and operation of the instrument. Some of the simulations used in this work have been performed on the Joint Fermilab-KICP Supercomputing Cluster. NR 42 TC 66 Z9 66 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD JUN 20 PY 2009 VL 698 IS 2 BP L133 EP L137 DI 10.1088/0004-637X/698/2/L133 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 458VB UT WOS:000267052600014 ER PT J AU Aptekar, RL Cline, TL Frederiks, DD Golenetskii, SV Mazets, EP Pal'shin, VD AF Aptekar, R. L. Cline, T. L. Frederiks, D. D. Golenetskii, S. V. Mazets, E. P. Pal'shin, V. D. TI KONUS-WIND OBSERVATIONS OF THE NEW SOFT GAMMA-RAY REPEATER SGR 0501+4516 SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE gamma rays: bursts; gamma rays: observations; pulsars: individual (SGR 0501+4516); stars: neutron ID BURST EMISSION; SGR-1806-20; DISCOVERY; MAGNETARS; DISTANCE; PULSAR; STARS AB In 2008 August, the new soft gamma-ray repeater SGR 0501+4516 was discovered by Swift. The source was soon confirmed by several groups in space-and ground-based multi-wavelength observations. In this Letter, we report the analysis of five short bursts from the recently discovered soft gamma-ray repeater (SGR), detected with the Konus Wind gamma-ray burst spectrometer. Properties of the time histories of the observed events, as well as results of multichannel spectral analysis, both in the 20-300 keV energy range, show, that the source exhibits itself as a typical SGR. The bursts durations are less than or similar to 0.75 s and their spectra above 20 keV can be fitted by an optically thin thermal bremsstrahlung (OTTB) model with kT(OTTB) of 20-40 keV. The spectral evolution is observed, which resembles the SGR 1627-41 bursts, where a strong hardness-intensity correlation was noticed in the earlier Konus-Wind observations. The peak energy fluxes of all five events are comparable to the highest of those for known SGRs, so a less distant source is implied, consistent with the determined Galactic anticenter direction. Supposing the young supernova remnant HB9 (at the distance of 1.5 kpc) as a natal environment of the source, the peak luminosities of the bursts are estimated to be (2-5) x 10(40) erg s(-1). The values of the total energy release, given the same assumptions, amount to (0.6-6)x10(39) erg. These estimations of both parameters are typical for short SGR bursts. C1 [Aptekar, R. L.; Frederiks, D. D.; Golenetskii, S. V.; Mazets, E. P.; Pal'shin, V. D.] Russian Acad Sci, AF Ioffe Physicotech Inst, St Petersburg 194021, Russia. [Cline, T. L.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Aptekar, RL (reprint author), Russian Acad Sci, AF Ioffe Physicotech Inst, St Petersburg 194021, Russia. RI Frederiks, Dmitry/C-7612-2014; Pal'shin, Valentin/F-3973-2014; Aptekar, Raphail/B-3456-2015; Golenetskii, Sergey/B-3818-2015; OI Frederiks, Dmitry/0000-0002-1153-6340 FU Federal Space Agency of Russia and RFBR [09-02-00166a] FX This work was supported by Federal Space Agency of Russia and RFBR grant 09-02-00166a. We gratefully acknowledge an anonymous referee for the detailed comments and suggestions, which have significantly improved this Letter. NR 39 TC 19 Z9 19 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD JUN 20 PY 2009 VL 698 IS 2 BP L82 EP L85 DI 10.1088/0004-637X/698/2/L82 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 458VB UT WOS:000267052600002 ER PT J AU Tavani, M Sabatini, S Pian, E Bulgarelli, A Caraveo, P Viotti, RF Corcoran, MF Giuliani, A Pittori, C Verrecchia, F Vercellone, S Mereghetti, S Argan, A Barbiellini, G Boffelli, F Cattaneo, PW Chen, AW Cocco, V D'Ammando, F Costa, E De Paris, G Del Monte, E Di Cocco, G Donnarumma, I Evangelista, Y Ferrari, A Feroci, M Fiorini, M Froysland, T Fuschino, F Galli, M Gianotti, F Labanti, C Lapshov, I Lazzarotto, F Lipari, P Longo, F Marisaldi, M Mastropietro, M Morelli, E Moretti, E Morselli, A Pacciani, L Pellizzoni, A Perotti, F Piano, G Picozza, P Pilia, M Porrovecchio, G Pucella, G Prest, M Rapisarda, M Rappoldi, A Rubini, A Soffitta, P Trifoglio, M Trois, A Vallazza, E Vittorini, V Zambra, A Zanello, D Santolamazza, P Giommi, P Colafrancesco, S Antonelli, LA Salotti, L AF Tavani, M. Sabatini, S. Pian, E. Bulgarelli, A. Caraveo, P. Viotti, R. F. Corcoran, M. F. Giuliani, A. Pittori, C. Verrecchia, F. Vercellone, S. Mereghetti, S. Argan, A. Barbiellini, G. Boffelli, F. Cattaneo, P. W. Chen, A. W. Cocco, V. D'Ammando, F. Costa, E. De Paris, G. Del Monte, E. Di Cocco, G. Donnarumma, I. Evangelista, Y. Ferrari, A. Feroci, M. Fiorini, M. Froysland, T. Fuschino, F. Galli, M. Gianotti, F. Labanti, C. Lapshov, I. Lazzarotto, F. Lipari, P. Longo, F. Marisaldi, M. Mastropietro, M. Morelli, E. Moretti, E. Morselli, A. Pacciani, L. Pellizzoni, A. Perotti, F. Piano, G. Picozza, P. Pilia, M. Porrovecchio, G. Pucella, G. Prest, M. Rapisarda, M. Rappoldi, A. Rubini, A. Soffitta, P. Trifoglio, M. Trois, A. Vallazza, E. Vittorini, V. Zambra, A. Zanello, D. Santolamazza, P. Giommi, P. Colafrancesco, S. Antonelli, L. A. Salotti, L. TI DETECTION OF GAMMA-RAY EMISSION FROM THE ETA-CARINAE REGION SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE gamma rays: observations; stars: individual (Eta Carinae); stars: winds, outflows; X-rays: binaries ID AGILE SILICON TRACKER; COLLIDING WINDS; LIGHT-CURVE; BEPPOSAX; BINARIES; EVENTS; SPACE; STARS; WR-25 AB We present the results of extensive observations by the gamma-ray AGILE satellite of the Galactic region hosting the Carina nebula and the remarkable colliding wind binary Eta Carinae (eta Car) during the period 2007 July-2009 January. We detect a gamma-ray source (1AGL J1043-5931) consistent with the position of eta Car. If 1AGL J1043-5931 is associated with the Car system, our data provide the long sought first detection above 100 MeV of a colliding wind binary. The average gamma-ray flux above 100 MeV and integrated over the preperiastron period 2007 July-2008 October is F(gamma) = (37 +/- 5) x 10(-8) ph cm(-2) s(-1) corresponding to an average gamma-ray luminosity of L(gamma) = 3.4 x 10(34) erg s(-1) for a distance of 2.3 kpc. We also report a two-day gamma-ray flaring episode of 1AGL J1043-5931 on 2008 October 11-13 possibly related to a transient acceleration and radiation episode of the strongly variable shock in the system. C1 [Tavani, M.; Argan, A.; Cocco, V.; D'Ammando, F.; Costa, E.; De Paris, G.; Del Monte, E.; Donnarumma, I.; Evangelista, Y.; Feroci, M.; Lapshov, I.; Lazzarotto, F.; Pacciani, L.; Piano, G.; Porrovecchio, G.; Pucella, G.; Rubini, A.; Soffitta, P.; Trois, A.; Vittorini, V.] IASF Roma, INAF, I-00133 Rome, Italy. [Sabatini, S.; D'Ammando, F.; Froysland, T.; Piano, G.; Picozza, P.; Vittorini, V.] Univ Roma Tor Vergata, Dipartimento Fis, I-00133 Rome, Italy. [Pian, E.] Osserv Astron Trieste, I-34131 Trieste, Italy. [Bulgarelli, A.; Di Cocco, G.; Fuschino, F.; Gianotti, F.; Labanti, C.; Marisaldi, M.; Morelli, E.; Trifoglio, M.] IASF Bologna, INAF, I-40129 Bologna, Italy. [Caraveo, P.; Giuliani, A.; Vercellone, S.; Mereghetti, S.; Chen, A. W.; Fiorini, M.; Perotti, F.; Zambra, A.] IASF Milano, INAF, I-20133 Milan, Italy. [Corcoran, M. F.] CRESST, Greenbelt, MD 20771 USA. [Corcoran, M. F.] NASA, Goddard Space Flight Ctr, Univ Space Res Assoc, Greenbelt, MD 20771 USA. [Pittori, C.; Verrecchia, F.; Santolamazza, P.; Giommi, P.; Colafrancesco, S.] ASI Sci Data Ctr, I-00044 Rome, Italy. [Barbiellini, G.; Longo, F.; Moretti, E.; Vallazza, E.] Dipartimento Fis, I-34127 Trieste, Italy. [Barbiellini, G.; Longo, F.; Moretti, E.; Vallazza, E.] Ist Nazl Fis Nucl, I-34127 Trieste, Italy. [Boffelli, F.; Cattaneo, P. W.; Rappoldi, A.] Ist Nazl Fis Nucl, I-27100 Pavia, Italy. [Chen, A. W.; Ferrari, A.; Froysland, T.] CIFS Torino, I-10133 Turin, Italy. [Ferrari, A.] Univ Turin, Dipartimento Fis, Turin, Italy. [Galli, M.] ENEA, I-40129 Bologna, Italy. [Lipari, P.; Zanello, D.] INFN Roma La Sapienza, I-00185 Rome, Italy. [Mastropietro, M.] IMIP, CNR, Rome, Italy. [Morselli, A.; Piano, G.; Picozza, P.] INFN Roma Tor Vergata, I-00133 Rome, Italy. [Pellizzoni, A.] Osservatorio Astron Cagliari, INAF, I-09012 Capoterra, Italy. [Pilia, M.; Prest, M.] Univ Insubria, Dipartimento Fis, I-22100 Como, Italy. [Rapisarda, M.] ENEA, I-00044 Rome, Italy. [Antonelli, L. A.] Osserv Astron Roma, INAF, I-00040 Monte Porzio Catone, Italy. [Salotti, L.] Agenzia Spaziale Italiana, I-00198 Rome, Italy. RP Tavani, M (reprint author), IASF Roma, INAF, I-00133 Rome, Italy. RI Morselli, Aldo/G-6769-2011; Lazzarotto, Francesco/J-4670-2012; Trifoglio, Massimo/F-5302-2015; Pittori, Carlotta/C-7710-2016; OI Caraveo, Patrizia/0000-0003-2478-8018; PREST, MICHELA/0000-0003-3161-4454; Verrecchia, Francesco/0000-0003-3455-5082; Marisaldi, Martino/0000-0002-4000-3789; Vercellone, Stefano/0000-0003-1163-1396; MEREGHETTI, SANDRO/0000-0003-3259-7801; Tavani, Marco/0000-0003-2893-1459; Pian, Elena/0000-0001-8646-4858; Soffitta, Paolo/0000-0002-7781-4104; Picozza, Piergiorgio/0000-0002-7986-3321; Fuschino, Fabio/0000-0003-2139-3299; Gianotti, Fulvio/0000-0003-4666-119X; Lazzarotto, Francesco/0000-0003-4871-4072; Costa, Enrico/0000-0003-4925-8523; Fiorini, Mauro/0000-0001-8297-1983; Bulgarelli, Andrea/0000-0001-6347-0649; giommi, paolo/0000-0002-2265-5003; Donnarumma, Immacolata/0000-0002-4700-4549; Pellizzoni, Alberto Paolo/0000-0002-4590-0040; Sabatini, Sabina/0000-0003-2076-5767; Morselli, Aldo/0000-0002-7704-9553; Trifoglio, Massimo/0000-0002-2505-3630; Pittori, Carlotta/0000-0001-6661-9779; Cattaneo, Paolo Walter/0000-0001-6877-6882; trois, alessio/0000-0002-3180-6002; galli, marcello/0000-0002-9135-3228; Pacciani, Luigi/0000-0001-6897-5996; Labanti, Claudio/0000-0002-5086-3619; Feroci, Marco/0000-0002-7617-3421 NR 26 TC 47 Z9 47 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD JUN 20 PY 2009 VL 698 IS 2 BP L142 EP L146 DI 10.1088/0004-637X/698/2/L142 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 458VB UT WOS:000267052600016 ER PT J AU Yamaleev, NK Carpenter, MH AF Yamaleev, Nail K. Carpenter, Mark H. TI A systematic methodology for constructing high-order energy stable WENO schemes SO JOURNAL OF COMPUTATIONAL PHYSICS LA English DT Article DE High-order finite difference methods; Weighted essentially non-oscillatory schemes; Energy estimate; Numerical stability; Artificial dissipation ID ESSENTIALLY NONOSCILLATORY SCHEMES; FINITE-DIFFERENCE APPROXIMATIONS; SCALAR CONSERVATION-LAWS; CONVERGENCE; EQUATIONS AB A third-order Energy Stable Weighted Essentially Non-Oscillatory (ESWENO) finite difference scheme developed by the authors of this paper [N.K Yamaleev, M.H. Carpenter, Third-order energy stable WENO scheme, J. Comput. Phys. 228 (2009) 3025-3047] was proven to be stable in the energy norm for both continuous and discontinuous solutions of systems of linear hyperbolic equations. Herein, a systematic approach is presented that enables "energy stable" modifications for existing WENO schemes of any order. The technique is demonstrated by developing a one-parameter family of fifth-order upwind-biased ESWENO schemes including one sixth-order central scheme; ESWENO schemes up to eighth order are presented in the Appendix. We also develop new weight functions and derive constraints on their parameters, which provide consistency, much faster convergence of the high-order ESWENO schemes to their underlying linear schemes for smooth solutions with arbitrary number of vanishing derivatives, and better resolution near strong discontinuities than the conventional counterparts. (C) 2009 Elsevier Inc. All rights reserved. C1 [Yamaleev, Nail K.] N Carolina Agr & Tech State Univ, Dept Math, Greensboro, NC 27411 USA. [Carpenter, Mark H.] NASA, Langley Res Ctr, Computat Aerosci Branch, Hampton, VA 23681 USA. RP Yamaleev, NK (reprint author), N Carolina Agr & Tech State Univ, Dept Math, Greensboro, NC 27411 USA. EM nkyamale@ncat.edu NR 15 TC 34 Z9 36 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 0021-9991 J9 J COMPUT PHYS JI J. Comput. Phys. PD JUN 20 PY 2009 VL 228 IS 11 BP 4248 EP 4272 DI 10.1016/j.jcp.2009.03.002 PG 25 WC Computer Science, Interdisciplinary Applications; Physics, Mathematical SC Computer Science; Physics GA 447DS UT WOS:000266172400017 ER PT J AU Field, CV Schmidt, GA AF Field, Christy V. Schmidt, Gavin A. TI Model-based constraints on interpreting 20th century trends in ice core Be-10 SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID COSMOGENIC-NUCLIDE PRODUCTION; SOLAR-ACTIVITY; DRY DEPOSITION; SOUTH-POLE; RECORDS; ACCUMULATION; SIMULATIONS; VARIABILITY; MODULATION; CLIMATE AB Beryllium-10 ice-core records are useful for understanding solar magnetic field changes over time, and in particular over the 20th century, during which there are a variety of relevant observations. However, differences between Be-10 snow concentration records from different locations complicate the process of developing a coherent understanding of changes in cosmogenic isotope production. We use the Goddard Institute for Space Studies ModelE general circulation model to simulate the production and transport of beryllium isotopes for this time period. We compare our results with surface air observations, and with ice-core records from Dye 3, Taylor Dome, and South Pole. We find that unforced weather-related (internal) variability causes modeled trends in (10) Be snow concentration to vary from the ensemble mean by 50% and greater at all three ice-core locations. Lower levels of internal variability at Taylor Dome and South Pole relative to Dye 3 make the simulated Be-10 values at these locations better estimates of the ensemble-mean trend in (10) Be snow concentration. In addition, the ensemble mean concentration trend at Dye 3 was significantly different from the expected modeled trend based on applied production changes alone. Overall, the results imply that during the 20th century, (10) Be data from multiple cores are likely to be required to make meaningful inferences about (10) Be production changes. The model simulations imply that data from Antarctica are likely to be more robust. C1 [Field, Christy V.] Columbia Univ, Dept Earth & Environm Sci, New York, NY 10027 USA. [Field, Christy V.; Schmidt, Gavin A.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA. [Schmidt, Gavin A.] Columbia Univ, Ctr Climate Syst Res, New York, NY USA. RP Field, CV (reprint author), Columbia Univ, Dept Earth & Environm Sci, New York, NY 10027 USA. EM cfield@giss.nasa.gov RI Schmidt, Gavin/D-4427-2012 OI Schmidt, Gavin/0000-0002-2258-0486 FU NSF [ATM-0317562]; U.S. National Science Foundation; Columbia University FX We would verymuch like to thank to Ju"rgBeer for his many helpful comments and for supplying 10 Be and 7 Be production functions. Two anonymous reviewers also helped improve the manuscript substantially. Thanks to Raimund Muscheler for the reconstructed f values, and to EML/SASP (http://www.eml.st.dhs.gov/databases/sasp/sasp_data_search.htm) for providing the 7 Be data. Support for this project was provided by NSF grant ATM-0317562. Christy Field also acknowledges support from the U.S. National Science Foundation through a Fellowship in the IGERT Joint Program in Applied Mathematics and Earth and Environmental Sciences at Columbia University. NR 46 TC 8 Z9 8 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 JUN 20 PY 2009 VL 114 AR D12110 DI 10.1029/2008JD011217 PG 11 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 460KU UT WOS:000267187400001 ER PT J AU Remsberg, EE AF Remsberg, Ellis E. TI Trends and solar cycle effects in temperature versus altitude from the Halogen Occultation Experiment for the mesosphere and upper stratosphere SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID MIDDLE ATMOSPHERE; LOWER THERMOSPHERE; VARIABILITY; SIMULATIONS; CO2 AB Fourteen-year time series of mesospheric and upper stratospheric temperature versus altitude or T(z) from the Halogen Occultation Experiment (HALOE) are analyzed and reported. The data have been binned according to 10 degrees-wide latitude zones from 40 degrees S to 40 degrees N and at 10 altitudes from 43 to 80 km: a total of 90 separate time series. Multiple linear regression analysis techniques have been applied to those time series. This study focuses on resolving their 11-year solar cycle (SC) (or SC-like) responses and their linear trend terms. Findings for T(z) from HALOE are compared with published results from ground-based Rayleigh lidar and from rocketsonde measurements. SC-like responses from HALOE compare well with those from the lidar station data. The cooling trends from HALOE also agree reasonably well with those from the lidar data at low latitudes for the concurrent decade. Cooling trends of the lower mesosphere from HALOE are not as large as those from rocketsondes and from the lidar station time series of the previous two decades, presumably because the changes in the upper stratospheric ozone are near zero during the HALOE time period and do not contribute to its trends. C1 NASA, Langley Res Ctr, Sci Directorate, Hampton, VA 23681 USA. RP Remsberg, EE (reprint author), NASA, Langley Res Ctr, Sci Directorate, 21 Langley Blvd,Mail Stop 401B, Hampton, VA 23681 USA. EM ellis.e.remsberg@nasa.gov NR 31 TC 26 Z9 26 U1 0 U2 1 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 JUN 20 PY 2009 VL 114 AR D12303 DI 10.1029/2009JD011897 PG 8 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 460KU UT WOS:000267187400002 ER PT J AU Wolff, MJ Smith, MD Clancy, RT Arvidson, R Kahre, M Seelos, F Murchie, S Savijarvi, H AF Wolff, M. J. Smith, M. D. Clancy, R. T. Arvidson, R. Kahre, M. Seelos, F. Murchie, S. Savijarvi, H. TI Wavelength dependence of dust aerosol single scattering albedo as observed by the Compact Reconnaissance Imaging Spectrometer SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Article ID MARTIAN ATMOSPHERE; PARTICLE SIZES; MARS; ABSORPTION; PATHFINDER; SURFACE; IMAGER AB Observations by the Compact Reconnaissance Imaging Spectrometer (CRISM) onboard the Mars Reconnaissance Orbiter (MRO) over the range 440-2920 nm of the very dusty Martian atmosphere of the 2007 planet-encircling dust event are combined with those made by both Mars Exploration Rovers (MERs) to better characterize the single scattering albedo (omega(0)) of Martian dust aerosols. Using the diagnostic geometry of the CRISM emission phase function (EPF) sequences and the "ground truth'' connection provided at both MER locations allows one to more effectively isolate the single scattering albedo (omega(0)). This approach eliminates a significant portion of the type of uncertainty involved in many of the earlier radiative transfer analyses. Furthermore, the use of a "first principles'' or microphysical representation of the aerosol scattering properties offers a direct path to produce a set of complex refractive indices (m = n + ik) that are consistent with the retrieved omega(0) values. We consider a family of effective particle radii: 1.2, 1.4, 1.6, and 1.8 mu m. The resulting set of model data comparisons, omega(0), and m are presented along with an assessment of potential sources of error and uncertainty. We discuss our results within the context of previous work, including the apparent dichotomy of the literature values: "dark'' (solar band omega(0) = 0.89-0.90) and "bright'' (solar band omega(0) = 0.92-0.94). Previous work suggests that a mean radius of 1.8 mu m is representative for the conditions sampled by the CRISM observations. Using the m for this case and a smaller effective particle radius more appropriate for diffuse dust conditions (1.4 mu m), we examine EPF-derived optical depths relative to the MER 880 nm optical depths. Finally, we explore the potential impact of the resulting brighter solar band omega(0) of 0.94 to atmospheric temperatures in the planetary boundary layer. C1 [Wolff, M. J.; Clancy, R. T.] Space Sci Inst, Boulder, CO 80301 USA. [Smith, M. D.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Arvidson, R.] Washington Univ, Dept Earth & Planetary Sci, St Louis, MO 63130 USA. [Kahre, M.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Seelos, F.; Murchie, S.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA. [Savijarvi, H.] Univ Helsinki, Dept Phys, FIN-00014 Helsinki, Finland. RP Wolff, MJ (reprint author), Space Sci Inst, 4750 Walnut St,Suite 205, Boulder, CO 80301 USA. EM mjwolff@spacescience.org RI Smith, Michael/C-8875-2012; Murchie, Scott/E-8030-2015; Seelos, Frank/C-7875-2016 OI Murchie, Scott/0000-0002-1616-8751; Seelos, Frank/0000-0001-9721-941X FU NASA FX We thank Jeff Johnson for helpful discussion regarding the application of his MER surface photometry to the different scales sampled by the CRISM footprint. We also thank Mathieu Vincendon for his insightful comments and suggestions. The authors also wish to acknowledge the financial support of NASA as members of the CRISM Science Team (via the Applied Physics Laboratory), without which this research would not have been possible. NR 49 TC 74 Z9 74 U1 2 U2 14 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9097 EI 2169-9100 J9 J GEOPHYS RES-PLANET JI J. Geophys. Res.-Planets PD JUN 20 PY 2009 VL 114 AR E00D04 DI 10.1029/2009JE003350 PG 17 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 460LY UT WOS:000267190400002 ER PT J AU Cui, J Galand, M Yelle, RV Vuitton, V Wahlund, JE Lavvas, PP Muller-Wodarg, ICF Cravens, TE Kasprzak, WT Waite, JH AF Cui, J. Galand, M. Yelle, R. V. Vuitton, V. Wahlund, J. -E. Lavvas, P. P. Mueller-Wodarg, I. C. F. Cravens, T. E. Kasprzak, W. T. Waite, J. H., Jr. TI Diurnal variations of Titan's ionosphere SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article ID PHOTOIONIZATION CROSS-SECTIONS; MASS-SPECTROMETER MEASUREMENTS; UPPER-ATMOSPHERE; CASSINI ION; GENERAL-CIRCULATION; MODEL; IONIZATION; CHEMISTRY; TEMPERATURE; OCCULTATION AB We present our analysis of the diurnal variations of Titan's ionosphere (between 1000 and 1300 km) based on a sample of Ion Neutral Mass Spectrometer (INMS) measurements in the Open Source Ion (OSI) mode obtained from eight close encounters of the Cassini spacecraft with Titan. Although there is an overall ion depletion well beyond the terminator, the ion content on Titan's nightside is still appreciable, with a density plateau of similar to 700 cm(-3) below similar to 1300 km. Such a plateau is a combined result of significant depletion of light ions and modest depletion of heavy ones on Titan's nightside. We propose that the distinctions between the diurnal variations of light and heavy ions are associated with their different chemical loss pathways, with the former primarily through "fast'' ion-neutral chemistry and the latter through "slow'' electron dissociative recombination. The strong correlation between the observed night-to-day ion density ratios and the associated ion lifetimes suggests a scenario in which the ions created on Titan's dayside may survive well to the nightside. The observed asymmetry between the dawn and dusk ion density profiles also supports such an interpretation. We construct a time-dependent ion chemistry model to investigate the effect of ion survival associated with solid body rotation alone as well as superrotating horizontal winds. For long-lived ions, the predicted diurnal variations have similar general characteristics to those observed. However, for short-lived ions, the model densities on the nightside are significantly lower than the observed values. This implies that electron precipitation from Saturn's magnetosphere may be an additional and important contributor to the densities of the short-lived ions observed on Titan's nightside. C1 [Cui, J.; Galand, M.; Mueller-Wodarg, I. C. F.] Univ London Imperial Coll Sci Technol & Med, Dept Phys, Space & Atmospher Phys Grp, London SW7 2BW, England. [Yelle, R. V.; Lavvas, P. P.] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA. [Vuitton, V.] Univ Grenoble 1, CNRS, Lab Planetol Grenoble, F-38041 Grenoble, France. [Wahlund, J. -E.] Swedish Inst Space Phys, Uppsala Div, SE-75121 Uppsala, Sweden. [Cravens, T. E.] Univ Kansas, Dept Phys & Astron, Lawrence, KS 66045 USA. [Kasprzak, W. T.] NASA, Goddard Space Flight Ctr, Solar Syst Explorat Div, Greenbelt, MD 20771 USA. [Waite, J. H., Jr.] SW Res Inst, Space Sci & Engn Div, San Antonio, TX 78238 USA. RP Cui, J (reprint author), Univ London Imperial Coll Sci Technol & Med, Dept Phys, Space & Atmospher Phys Grp, Prince Consort Rd, London SW7 2BW, England. EM j.cui@imperial.ac.uk RI Galand, Marina/C-6804-2009; Mueller-Wodarg, Ingo/M-9945-2014 OI Mueller-Wodarg, Ingo/0000-0001-6308-7826 FU NASA [NAG5-12699]; University of Arizona [699083KC]; University Research Fellowship of the British Royal Society; Jet Propulsion Laboratory [1283095] FX J. C. and M. G. are supported by the Science and Technology Facilities Council (STFC) rolling grant to Imperial College London. R. V. Y. and P. P. L. acknowledge the support from NASA through grant NAG5-12699 to the University of Arizona and subcontract 699083KC from the Southwest Research Institute. I. M.-W. is funded by a University Research Fellowship of the British Royal Society. J. H. W. is funded by NASA and the Jet Propulsion Laboratory contract 1283095 with Southwest Research Institute. NR 55 TC 45 Z9 45 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 JUN 18 PY 2009 VL 114 AR A06310 DI 10.1029/2009JA014228 PG 20 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 460MF UT WOS:000267191100003 ER PT J AU Lyatskaya, S Lyatsky, W Khazanov, GV AF Lyatskaya, Sonya Lyatsky, W. Khazanov, G. V. TI Auroral electrojet AL index and polar magnetic disturbances in two hemispheres SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article ID FIELD-ALIGNED CURRENTS; GEOMAGNETIC-ACTIVITY; CAP AB Earlier we found that the auroral electrojet AL index, indicating substorm activity in the northern hemisphere, in local summer months correlates much better with geomagnetic activity not in the nearby polar cap but in the opposite polar cap; we explained this effect as a result of interhemispheric field-aligned currents, which suppress substorm field-aligned currents in the summer hemisphere but increase these currents in the winter hemisphere. In the present paper, we took into account this effect and examined a method for reliably monitoring the substorm auroral electrojet, measured with the auroral electrojet AL index, by using hourly averages of geomagnetic field from two polar observatories (Thule and Vostok) in two hemispheres. We tested this method for 3 years. The correlation between the predicted and actual AL indices for these years was stable and very high, and it showed no significant dependence on season and a relatively weak UT variation. The correlation coefficient between the predicted and actual AL indices for these three years was about 0.89. The proposed method, based on using magnetic field data from two polar geomagnetic observatories in two hemispheres, not only significantly improves the reliability of monitoring the westward auroral electrojet in the northern hemisphere but it may also be used for monitoring the westward auroral electrojet in the southern hemisphere where no AL index is available because a significant portion of the southern auroral zone is located over the oceans. The results of this paper show that measurements of geomagnetic field in two hemispheres are of high importance for reliably monitoring the geomagnetic activity and related events in each hemisphere. C1 [Lyatskaya, Sonya] Alabama A&M Univ, Dept Phys, Normal, AL 35762 USA. [Lyatsky, W.; Khazanov, G. V.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Lyatskaya, S (reprint author), Alabama A&M Univ, Dept Phys, 4900 Meridian St, Normal, AL 35762 USA. EM sonya.lyatskaya@gmail.com RI feggans, john/F-5370-2012 FU NASA; NASA/MSFC FX We gratefully acknowledge efforts of the staff of the World Data Center for Geomagnetism in Kyoto, Japan, and World Data Center for Geomagnetism in Copenhagen, Denmark, in providing geomagnetic data from high-latitude geomagnetic observatories. This research was performed while Wladislaw Lyatsky held a NASA Senior Postdoctoral Program appointment at NASA/MSFC. Funding in support of this study was provided partially by the NASA HQ POLAR Project and the NASA LWS Program. NR 20 TC 6 Z9 6 U1 0 U2 2 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0148-0227 J9 J GEOPHYS RES-SPACE JI J. Geophys. Res-Space Phys. PD JUN 18 PY 2009 VL 114 AR A06212 DI 10.1029/2009JA014100 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 460MF UT WOS:000267191100001 ER PT J AU Taguchi, S Suzuki, S Hosokawa, K Ogawa, Y Yukimatu, AS Sato, N Collier, MR Moore, TE AF Taguchi, S. Suzuki, S. Hosokawa, K. Ogawa, Y. Yukimatu, A. S. Sato, N. Collier, M. R. Moore, T. E. TI Moving mesoscale plasma precipitation in the cusp SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article ID LOW-ALTITUDE OBSERVATIONS; FLUX-TRANSFER EVENTS; SOLAR-WIND; MAGNETIC-FIELD; DAYSIDE MAGNETOPAUSE; MAGNETOSPHERIC CUSP; NEUTRAL ATOMS; RECONNECTION; CONVECTION; SPACECRAFT AB On 28 March 2001, when the interplanetary magnetic field was strongly duskward, the DMSP F12 spacecraft observed an ion precipitation burst in a latitudinally narrow region near 1200 MLT. A few minutes earlier, the Low Energy Neutral Atom (LENA) imager on the IMAGE spacecraft, whose field of view (FOV) looks into the high-altitude cusp, detected an enhancement of energetic neutral atom signals, which are produced by the ion injection. The LENA data suggest that the ion injection moved out of its FOV after approximately 4 min. At this time, the ground-based magnetometers of the IMAGE chain in Svalbard, located westward of LENA's FOV, began to indicate perturbations. These perturbations immediately reached a peak and then ceased; the perturbations lasted 2-3 min. During this interval, there was an enhanced westward flow over Svalbard, as observed by the SuperDARN radars. The EISCAT Svalbard radar detected an enhancement of electron density and temperature that was concurrent with this flow enhancement, suggesting that a plasma precipitation burst accompanied with the flow. These observations, which cover a longitudinally extending region of the cusp, strongly suggest the existence of moving mesoscale plasma precipitation (MMPP). The MMPP travels westward with a longitudinally elongated form. Its leading and trailing edges should be created by the temporal effect of the cusp. The other edges, which lie along the streamline, would originate in a spatially limited region along the open-closed line. The boundary of the MMPP form is delineated by both the temporal and spatial structures of the cusp. C1 [Taguchi, S.; Hosokawa, K.] Univ Electrocommun, Dept Informat & Commun Engn, Tokyo 1828585, Japan. [Suzuki, S.] Univ Electrocommun, Sugadaira Space Radio Observ, Tokyo 1828585, Japan. [Ogawa, Y.; Yukimatu, A. S.; Sato, N.] Natl Inst Polar Res, Tokyo 1738515, Japan. [Collier, M. R.; Moore, T. E.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Taguchi, S (reprint author), Univ Electrocommun, Dept Informat & Commun Engn, 1-5-1 Chofugaoka, Tokyo 1828585, Japan. EM taguchi@ice.uec.ac.jp RI Moore, Thomas/D-4675-2012; Collier, Michael/I-4864-2013 OI Moore, Thomas/0000-0002-3150-1137; Collier, Michael/0000-0001-9658-6605 FU Japan Society for the Promotion of Science [18540443]; National Institute of Polar Research collaboration [20-7]; IMAGE Project [UPN 370-28-20]; JHU/APL FX This research was supported by Grant-in-Aid for Scientific Research (C) 18540443 under Japan Society for the Promotion of Science, by National Institute of Polar Research collaboration project 20-7, and by the IMAGE Project under UPN 370-28-20 at Goddard Space Flight Center. The DMSP particle detectors were designed by David Hardy of AFRL, and data were obtained from JHU/APL. We thank David Hardy, Fred Rich, and Patrick Newell for its use. We also thank the NR 49 TC 6 Z9 6 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 JUN 18 PY 2009 VL 114 AR A06211 DI 10.1029/2009JA014128 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 460MF UT WOS:000267191100002 ER PT J AU LaHaye, MD Suh, J Echternach, PM Schwab, KC Roukes, ML AF LaHaye, M. D. Suh, J. Echternach, P. M. Schwab, K. C. Roukes, M. L. TI Nanomechanical measurements of a superconducting qubit SO NATURE LA English DT Article ID RESONATOR; STATES; PHASE AB The observation of the quantum states of motion of a macroscopic mechanical structure remains an open challenge in quantum-state preparation and measurement. One approach that has received extensive theoretical attention(1-13) is the integration of superconducting qubits as control and detection elements in nanoelectromechanical systems (NEMS). Here we report measurements of a NEMS resonator coupled to a superconducting qubit, a Cooper-pair box. We demonstrate that the coupling results in a dispersive shift of the nanomechanical frequency that is the mechanical analogue of the 'single-atom index effect'(14) experienced by electromagnetic resonators in cavity quantum electrodynamics. The large magnitude of the dispersive interaction allows us to perform NEMS-based spectroscopy of the superconducting qubit, and enables observation of Landau-Zener interference effects-a demonstration of nanomechanical read-out of quantum interference. C1 [LaHaye, M. D.; Suh, J.; Roukes, M. L.] CALTECH, Kavli Nanosci Inst, Pasadena, CA 91125 USA. [Echternach, P. M.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Roukes, ML (reprint author), CALTECH, Kavli Nanosci Inst, MS 114-36, Pasadena, CA 91125 USA. EM roukes@caltech.edu RI Roukes, Michael/E-9787-2010; OI Suh, Junho/0000-0002-0112-0499; LaHaye, Matthew/0000-0003-1911-0704 FU US National Science Foundation [DMR-0804567]; Foundational Questions Institute [RFP2-08-27]; Center for the Physics of Information, California Institute of Technology; US National Aeronautics and Space Administration FX The authors would like to thank T. Duty, C. Wilson, G. Milburn, A. Doherty, E. Babourina-Brooks, A. Armour, A. Clerk and I. Bargatin for discussions; S. Stryker and A. Sears for assistance in constructing the measurement apparatus; and R. E. Muller for electron beam lithography. K. C. S. acknowledges support from the US National Science Foundation (DMR-0804567) and the Foundational Questions Institute (RFP2-08-27). M. D. L. acknowledges support from the Center for the Physics of Information, California Institute of Technology. Part of the research described in this publication was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the US National Aeronautics and Space Administration. NR 30 TC 190 Z9 194 U1 2 U2 27 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 0028-0836 EI 1476-4687 J9 NATURE JI Nature PD JUN 18 PY 2009 VL 459 IS 7249 BP 960 EP 964 DI 10.1038/nature08093 PG 5 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 458XS UT WOS:000267063500037 PM 19536259 ER PT J AU Wright, JS Sobel, AH Schmidt, GA AF Wright, Jonathon S. Sobel, Adam H. Schmidt, Gavin A. TI Influence of condensate evaporation on water vapor and its stable isotopes in a GCM SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID LARGE-SCALE ADVECTION; SUBTROPICAL HUMIDITY; PRECIPITATION; CONVECTION AB The direct effect of condensate evaporation on atmospheric water vapor and its isotopic composition is assessed in a climate model. The model contains two parallel hydrologic cycles, an active one which influences the model physics and dynamics and a passive one which does not. Two model simulations are performed, one in which passive cloud and precipitation can evaporate and one in which they cannot. The active hydrologic cycles, and thus the simulated circulations and temperatures, are identical in both simulations. Eliminating passive condensate evaporation reduces the specific humidity in the passive cycle by around 5%; this reduction varies from a few percent to 25% of the control value, depending on location. Zonal mean water vapor in the lower and middle troposphere is enriched in HDO relative to the control case, and is depleted in the upper troposphere. Citation: Wright, J. S., A. H. Sobel, and G. A. Schmidt (2009), Influence of condensate evaporation on water vapor and its stable isotopes in a GCM, Geophys. Res. Lett., 36, L12804, doi:10.1029/2009GL038091. C1 [Wright, Jonathon S.; Sobel, Adam H.] Columbia Univ, Dept Appl Phys & Appl Math, New York, NY 10027 USA. [Schmidt, Gavin A.] Columbia Univ, NASA, Goddard Inst Space Studies, New York, NY 10025 USA. [Schmidt, Gavin A.] Columbia Univ, Ctr Climate Syst Res, New York, NY 10025 USA. RP Wright, JS (reprint author), Columbia Univ, Dept Appl Phys & Appl Math, 500 W 120th St,Room 200, New York, NY 10027 USA. EM jw2519@columbia.edu; ahs129@columbia.edu; gschmidt@giss.nasa.gov RI Schmidt, Gavin/D-4427-2012; Sobel, Adam/K-4014-2015; OI Schmidt, Gavin/0000-0002-2258-0486; Sobel, Adam/0000-0003-3602-0567; Wright, Jonathon/0000-0001-6551-7017 FU NASA [NNX06AB01G]; NSF [ATM-0542736] FX J. Wright and A. Sobel thank Joe Galewsky for useful discussions and Paul Wennberg for stimulating our interest in isotopes. This work was supported by NASA grant NNX06AB01G and NSF grant ATM-0542736. NR 17 TC 21 Z9 21 U1 1 U2 8 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD JUN 17 PY 2009 VL 36 AR L12804 DI 10.1029/2009GL038091 PG 5 WC Geosciences, Multidisciplinary SC Geology GA 460KF UT WOS:000267185900004 ER PT J AU Madsen, MB Goetz, W Bertelsen, P Binau, CS Folkmann, F Gunnlaugsson, HP Hjollum, JI Hviid, SF Jensen, J Kinch, KM Leer, K Madsen, DE Merrison, J Olsen, M Arneson, HM Bell, JF Gellert, R Herkenhoff, KE Johnson, JR Johnson, MJ Klingelhofer, G McCartney, E Ming, DW Morris, RV Proton, JB Rodionov, D Sims, M Squyres, SW Wdowiak, T Yen, AS AF Madsen, M. B. Goetz, W. Bertelsen, P. Binau, C. S. Folkmann, F. Gunnlaugsson, H. P. Hjollum, J. I. Hviid, S. F. Jensen, J. Kinch, K. M. Leer, K. Madsen, D. E. Merrison, J. Olsen, M. Arneson, H. M. Bell, J. F., III Gellert, R. Herkenhoff, K. E. Johnson, J. R. Johnson, M. J. Klingelhoefer, G. McCartney, E. Ming, D. W. Morris, R. V. Proton, J. B. Rodionov, D. Sims, M. Squyres, S. W. Wdowiak, T. Yen, A. S. TI Overview of the magnetic properties experiments on the Mars Exploration Rovers SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Article ID MARTIAN ATMOSPHERE; PATHFINDER; DUST; IMAGER; MINERALOGY; METEORITES; CHEMISTRY; MISSION; SPIRIT; LANDER AB The Mars Exploration Rovers have accumulated airborne dust on different types of permanent magnets. Images of these magnets document the dynamics of dust capture and removal over time. The strongly magnetic subset of airborne dust appears dark brown to black in Panoramic Camera (Pancam) images, while the weakly magnetic one is bright red. Images returned by the Microscopic Imager reveal the formation of magnetic chains diagnostic of magnetite-rich grains with substantial magnetization (>8 Am-2 kg(-1)). On the basis of Mossbauer spectra the dust contains magnetite, olivine, pyroxene, and nanophase oxides in varying proportions, depending on wind regime and landing site. The dust contains a larger amount of ferric iron (Fe3+/Fe-tot similar to 0.6) than rocks in the Gusev plains (similar to 0.1-0.2) or average Gusev soil (similar to 0.3). Alpha Particle X-Ray Spectrometer data of the dust show that some of the iron in magnetite is substituted by titanium and chromium. The good correlation of the amount of calcium and sulfur in the dust may be caused by the presence of a calcium sulfate related phase. The overall mineralogical composition points to a basaltic origin of the airborne dust, although some alteration has taken place as indicated by the large degree of oxidation. C1 [Madsen, M. B.; Bertelsen, P.; Binau, C. S.; Leer, K.; Olsen, M.] Univ Copenhagen, Niels Bohr Inst, DK-2100 Copenhagen, Denmark. [Goetz, W.; Hviid, S. F.] Max Planck Inst Sonnensyst Forsch, D-37191 Katlenburg Lindau, Germany. [Folkmann, F.; Gunnlaugsson, H. P.; Jensen, J.; Merrison, J.] Univ Aarhus, Inst Phys & Astron, DK-8000 Aarhus, Denmark. [Hjollum, J. I.] Tech Univ Denmark, Natl Lab Sustainable Energy, Mat Res Dept, DK-4000 Roskilde, Denmark. [Kinch, K. M.; Arneson, H. M.; Bell, J. F., III; Johnson, M. J.; McCartney, E.; Proton, J. B.; Squyres, S. W.] Cornell Univ, Dept Astron, Ithaca, NY 14853 USA. [Madsen, D. E.] Tech Univ Denmark, Dept Phys, DK-2800 Lyngby, Denmark. [Gellert, R.] Univ Guelph, Dept Phys, Guelph, ON N1G 2W1, Canada. [Herkenhoff, K. E.; Johnson, J. R.] US Geol Survey, Astrogeol Team, Flagstaff, AZ 86001 USA. [Klingelhoefer, G.; Rodionov, D.] Johannes Gutenberg Univ Mainz, D-55128 Mainz, Germany. [Ming, D. W.; Morris, R. V.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. [Sims, M.] NASA, Ames Res Ctr, Planetary Syst Branch, Div Space Sci, Moffett Field, CA 94035 USA. [Wdowiak, T.] Univ Alabama Birmingham, Dept Phys, Astro & Solar Syst Phys Program, Birmingham, AL 35294 USA. [Yen, A. S.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Madsen, MB (reprint author), Univ Copenhagen, Niels Bohr Inst, Blegdamsvej 17, DK-2100 Copenhagen, Denmark. EM mbmadsen@fys.ku.dk RI Madsen, Morten/D-2082-2011; Kinch, Kjartan/C-5742-2015; Johnson, Jeffrey/F-3972-2015; OI Madsen, Morten/0000-0001-8909-5111; Kinch, Kjartan/0000-0002-4629-8880; merrison, jonathan/0000-0003-4362-6356 FU Danish Science Agency; Thomas B. Thrige's foundation; DELTA Danish Electronics, Light & Acoustics in Horsholm, Denmark; University of Copenhagen FX Danish participation in the MER missions was supported by the Danish Science Agency, by Thomas B. Thrige's foundation, and by DELTA Danish Electronics, Light & Acoustics in Horsholm, Denmark. Support from the University of Copenhagen for C. S. B. and W. G. is gratefully acknowledged. The authors also thank Peter H. Smith, Lunar and Planetary Laboratory, the University of Arizona, as well as an anonymous reviewer for constructive and inspiring criticism on the manuscript. We are indebted to the scientists and engineers of the MER team for their continuous support which made these experiments possible. NR 46 TC 13 Z9 13 U1 3 U2 18 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 JUN 16 PY 2009 VL 114 AR E06S90 DI 10.1029/2008JE003098 PG 20 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 460LU UT WOS:000267190000001 ER PT J AU Allwood, AC Grotzinger, JP Knoll, AH Burch, IW Anderson, MS Coleman, ML Kanik, I AF Allwood, Abigail C. Grotzinger, John P. Knoll, Andrew H. Burch, Ian W. Anderson, Mark S. Coleman, Max L. Kanik, Isik TI Controls on development and diversity of Early Archean stromatolites SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF AMERICA LA English DT Article DE microbe; paleontology; biosignature; carbonate; reef ID WESTERN-AUSTRALIA; WARRAWOONA GROUP; PILBARA CRATON; CHERT; MICROFOSSILS; MODEL; LIFE; REEF AB The approximate to 3,450-million-year-old Strelley Pool Formation in Western Australia contains a reef-like assembly of laminated sedimentary accretion structures (stromatolites) that have macroscale characteristics suggestive of biological influence. However, direct microscale evidence of biology-namely, organic microbial remains or biosedimentary fabrics-has to date eluded discovery in the extensively-recrystallized rocks. Recently-identified outcrops with relatively good textural preservation record microscale evidence of primary sedimentary processes, including some that indicate probable microbial mat formation. Furthermore, we find relict fabrics and organic layers that covary with stromatolite morphology, linking morphologic diversity to changes in sedimentation, seafloor mineral precipitation, and inferred microbial mat development. Thus, the most direct and compelling signatures of life in the Strelley Pool Formation are those observed at the microscopic scale. By examining spatiotemporal changes in microscale characteristics it is possible not only to recognize the presence of probable microbial mats during stromatolite development, but also to infer aspects of the biological inputs to stromatolite morphogenesis. The persistence of an inferred biological signal through changing environmental circumstances and stromatolite types indicates that benthic microbial populations adapted to shifting environmental conditions in early oceans. C1 [Allwood, Abigail C.; Anderson, Mark S.; Coleman, Max L.; Kanik, Isik] CALTECH, Jet Prop Lab, NASA, Astrobiol Inst, Pasadena, CA 91109 USA. [Allwood, Abigail C.; Burch, Ian W.] Univ New S Wales, Australian Ctr Astrobiol, Sydney, NSW 2052, Australia. [Grotzinger, John P.] CALTECH, Dept Geol & Planetary Sci, Pasadena, CA 91125 USA. [Knoll, Andrew H.] Harvard Univ, Dept Organism & Evolut Biol, Cambridge, MA 02138 USA. RP Allwood, AC (reprint author), CALTECH, Jet Prop Lab, NASA, Astrobiol Inst, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM abigail.c.allwood@jpl.nasa.gov; grotz@gps.caltech.edu FU National Aeronautics and Space Administration (NASA); National Aeronautics and Space Administration FX We thank the Geological Survey of Western Australia for generous field support, Malcolm Walter and Arthur Hickman for helpful discussions, George Rossman for use of Caltech Raman Laboratory, and Dawn Sumner and Ian Fairchild for helpful reviews. Fieldwork was partly supported by the Agouron Institute. A. C. A. was supported by the National Aeronautics and Space Administration (NASA) Postdoctoral Program. The work of A. C. A., M. S. A., M. L. C., and I. K. was conducted at the Jet Propulsion Laboratory under contract to the National Aeronautics and Space Administration (with Research and Technology Program/Astrobiology Science and Technology for Exploring Planets funding). NR 32 TC 86 Z9 92 U1 4 U2 45 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 JUN 16 PY 2009 VL 106 IS 24 BP 9548 EP 9555 DI 10.1073/pnas.0903323106 PG 8 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 458TD UT WOS:000267045500004 PM 19515817 ER PT J AU Balk, M Bose, M Ertem, G Rogoff, DA Rothschild, LJ Freund, FT AF Balk, Melike Bose, Milton Ertem, Goezen Rogoff, Dana A. Rothschild, Lynn J. Freund, Friedernann T. TI Oxidation of water to hydrogen peroxide at the rock-water interface due to stress-activated electric currents in rocks SO EARTH AND PLANETARY SCIENCE LETTERS LA English DT Article DE hydrogen peroxide; rock-water interface; electric currents; rock battery; oxidation; early Earth; early life ID ATMOSPHERIC OXYGEN; MAGNESIUM-OXIDE; IGNEOUS ROCKS; PHOTOSYNTHESIS; SILICATES; NETWORKS; HOLES; EARTH; MGO; OH AB Common igneous and high-grade metamorphic rocks contain dormant defects, which release electronic charge carriers when stressed. Rocks thereby behave like a battery. The charge carriers of interest are defect electrons h(center dot), e.g. electronic states associated with O- in a matrix of O2-. Known as "positive holes" or pholes for short, the h(center dot) travel along stress gradients over distances on the order of meters in the laboratory and kilometers in the field. At rock-water interfaces the h(center dot) turn into center dot O radicals, e.g. highly reactive oxygen species, which oxidize H2O to H2O2. For every two h(center dot) charge carriers one H2O2 molecule is formed. In the laboratory the battery circuit is closed by running a Cu wire from the stressed to the unstressed rock In the field closure of the circuit may be provided through the electrolytical conductivity of water. The discovery of h(center dot) charge carriers, their stress-activation, and their effect on Earth's surface environment may help better understand the oxidation of the early Earth and the evolution of early life. (C) 2009 Elsevier B.V. All rights reserved. C1 [Rogoff, Dana A.; Freund, Friedernann T.] SETI Inst, Carl Sagan Ctr, Mountain View, CA 94043 USA. [Balk, Melike; Rothschild, Lynn J.; Freund, Friedernann T.] NASA, Ames Res Ctr, Code SGE, Moffett Field, CA 94035 USA. [Ertem, Goezen] NASA, Ames Res Ctr, Code SSX, Moffett Field, CA 94035 USA. [Bose, Milton; Freund, Friedernann T.] San Jose State Univ, Dept Phys, San Jose, CA 95192 USA. RP Freund, FT (reprint author), SETI Inst, Carl Sagan Ctr, 515 N Whisman Rd, Mountain View, CA 94043 USA. EM M.Balk@nioo.knaw.nl; milton.bose@gmail.com; gozen1ertem@gmail.com; drogoff@mail.arc.nasa.gov; Lynn.J.Rothschild@nasa.gov; friedemann.T.freund@nasa.gov FU NASA Astrobiology Institute (NAI) [NNA04CC05A]; Netherlands Organization for Scientific Research (NWO); National Research Council; Oak Ridge Associated Universities (ORAU) FX This work was supported in part by a grant from the NASA Astrobiology Institute (NAI) Cooperative Agreement NNA04CC05A (to F.T.F and LJ.R.). M. Balk acknowledges a travel grant from the Netherlands Organization for Scientific Research (NWO). G.E. acknowledges a NASA Senior Fellowship through the National Research Council and the Oak Ridge Associated Universities (ORAU). NR 43 TC 19 Z9 20 U1 1 U2 6 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 JUN 15 PY 2009 VL 283 IS 1-4 BP 87 EP 92 DI 10.1016/j.epsl.2009.03.044 PG 6 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 464OD UT WOS:000267513700009 ER PT J AU Eggenkamp, HGM Coleman, ML AF Eggenkamp, H. G. M. Coleman, M. L. TI The effect of aqueous diffusion on the fractionation of chlorine and bromine stable isotopes SO GEOCHIMICA ET COSMOCHIMICA ACTA LA English DT Article ID DURCH ELEKTROLYTISCHE UBERFUHRUNG; MOLECULAR-DYNAMICS SIMULATIONS; MASS-SPECTROMETRY; LIQUID WATER; SEDIMENTS; RATIOS; IONS; HYDRATION; CL-35; CLAY AB Diffusive isotopic fractionation factors are important in order to understand natural processes and have practical application in radioactive waste storage and carbon dioxide sequestration. We determined the isotope fractionation factors and the effective diffusion coefficients of chloride and bromide ions during aqueous diffusion in polyacrylamide gel. Diffusion was determined as functions of temperature, time and concentration. The effect of temperature is relatively large on the diffusion coefficient (D) but only small on isotope fractionation. For chlorine, the ratio, D-35cl/D-37cl varied from 1.00128 +/- 0.00017 (1 sigma) at 2 degrees C to 1.00192 +/- 0.00015 at 80 degrees C. For bromine, D-79Br/D-81Br varied from 1.00098 +/- 0.00009 at 2 degrees C to 1.0064 +/- 0.00013 at 21 degrees C and 1.00078 +/- 0.00018 (1 sigma) at 80 degrees C. There were no significant effects on the isotope fractionation due to concentration. The lack of sensitivity of the diffusive isotope fractionation to anything at the most common temperatures (0 to 30 C) makes it particularly valuable for application to understanding processes in geological environments and an important natural tracer in order to understand fluid transport processes. (C) 2009 Elsevier Ltd. All rights reserved. C1 [Eggenkamp, H. G. M.] Univ Tecn Lisboa, Ctr Petrol & Geoquim, Inst Super Tecn, P-1049001 Lisbon, Portugal. [Coleman, M. L.] CALTECH, NASA Astrobiol Inst, Pasadena, CA 91109 USA. [Coleman, M. L.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Eggenkamp, H. G. M.; Coleman, M. L.] Univ Reading, Postgrad Res Inst Sedimentol, Reading RG6 6AB, Berks, England. RP Eggenkamp, HGM (reprint author), Univ Tecn Lisboa, Ctr Petrol & Geoquim, Inst Super Tecn, Ave Rovisco Pais, P-1049001 Lisbon, Portugal. EM hermanus.eggenkamp@ist.utl.pt; max.coleman@jpl.nasa.gov RI Eggenkamp, Hans/C-4006-2008; Coleman, Max/A-1303-2007 OI Eggenkamp, Hans/0000-0001-5874-0157; Coleman, Max/0000-0002-5514-1826 FU UK Natural Environment Research Council [GR3/10360, 1996-1998]; NASA; JPL's Research and Technology Development Program [01STCR-R.07.023.011]; Portuguese Foundation for Science and Technology (FCT) FX We thank Dr. I.C. Bourg, two anonymous reviewers and the Associate Editor, Dr. J. Horita, for very helpful comments which improved the manuscript considerably. This work was enabled originally by a grant to MC a very long time ago from the UK Natural Environment Research Council (Controls on chemical compositions of basinal brines, GR3/10360, 1996-1998). The contribution of MC was carried out in part at the Jet Propulsion Laboratory (JPL), California Institute of Technology, under contract with the National Aeronautics and Space Administration (NASA) and partly supported by JPL's Research and Technology Development Program (Grant 01STCR-R.07.023.011). Part of the contribution of HE was funded by the Portuguese Foundation for Science and Technology (FCT) under the Ciencia 2007 program. This is PRIS Contribution N degrees 31, 416. NR 48 TC 33 Z9 35 U1 6 U2 42 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0016-7037 EI 1872-9533 J9 GEOCHIM COSMOCHIM AC JI Geochim. Cosmochim. Acta PD JUN 15 PY 2009 VL 73 IS 12 BP 3539 EP 3548 DI 10.1016/j.gca.2009.03.036 PG 10 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 451FF UT WOS:000266455400002 ER PT J AU Li, W Nahak, C AF Li, Wu Nahak, Chandal TI Regularized gap function as penalty term for constrained minimization problems SO JOURNAL OF MATHEMATICAL ANALYSIS AND APPLICATIONS LA English DT Article DE Regularized gap function; Constrained optimization; Unconstrained reformulation; Exact penalty function; Merit function; Invexity; Strong coerciveness; Bounded level set ID VARIATIONAL INEQUALITY PROBLEMS; UNCONSTRAINED MINIMIZATION; INVEXITY AB By using the regularized gap function for variational inequalities, Li and Peng introduced a new penalty function P(alpha)(x) for the problem of minimizing a twice continuously differentiable function in closed convex subset of the n-dimensional space R(n). Under certain assumptions, they proved that the original constrained minimization problem is equivalent to unconstrained minimization of P(alpha)(x). The main purpose of this paper is to give an in-depth study of those properties of the objective function that can be extended from the feasible set to the whole R(n) by P(alpha)(x). For example, it is proved that the objective function has bounded level sets (or is strongly coercive) on the feasible set if and only if P(alpha)(x) has bounded level sets (or is strongly coercive) on R(n). However, the convexity of the objective function does not imply the convexity of P(alpha)(x) when the objective function is not quadratic, no matter how small alpha is. Instead, the convexity of the objective function on the feasible set only implies the invexity of P(alpha)(x) on R(n). Moreover, a characterization for the invexity of P(alpha)(x) is also given. (C) 2009 Elsevier Inc. All rights reserved. C1 [Nahak, Chandal] Indian Inst Technol, Dept Math, Kharagpur 721302, W Bengal, India. [Li, Wu] NASA, Langley Res Ctr, Aeronaut Syst Anal Branch, Hampton, VA 23681 USA. RP Nahak, C (reprint author), Indian Inst Technol, Dept Math, Kharagpur 721302, W Bengal, India. EM w.li@nasa.gov; cnahak@maths.iitkgp.ernet.in FU CSIR, New Delhi [25(0163)/08/17MR-II] FX Partially supported by CSIR, New Delhi, grant 25(0163)/08/17MR-II. NR 15 TC 0 Z9 0 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 0022-247X J9 J MATH ANAL APPL JI J. Math. Anal. Appl. PD JUN 15 PY 2009 VL 354 IS 2 BP 575 EP 583 DI 10.1016/j.jmaa.2008.12.048 PG 9 WC Mathematics, Applied; Mathematics SC Mathematics GA 439VD UT WOS:000265654600019 ER PT J AU Hulley, GC Hook, SJ AF Hulley, Glynn C. Hook, Simon J. TI Intercomparison of versions 4, 4.1 and 5 of the MODIS Land Surface Temperature and Emissivity products and validation with laboratory measurements of sand samples from the Namib desert, Namibia SO REMOTE SENSING OF ENVIRONMENT LA English DT Article DE Emissivity; Land surface temperature; MODIS; Validation; Thermal infrared; Namib ID ALGORITHM AB Eight new refinements were implemented in the MODIS Land Surface Temperature and Emissivity (LST&E) product suite when transitioning from version 4 (W) to version 5 (V5). The refinements were designed to improve the spatial coverage, stability, and accuracy of the product suite. Version 4.1 (V4.1) is an interim collection which uses V5 input products (MOD02, MOD03, MOD07, MOD10, and MOD35), but the LST&E retrieval algorithm is unchanged from V4 in which the split-window and day/night temperature retrieval algorithms are only partially incorporated, and not fully incorporated as in V5. A test dataset for the V4.1 product was produced by MODAPS for a 3-month period from July through September 2004, and after an initial evaluation period, it was decided to generate the V4.1 product from mission period 2007001 onwards as a continuation of previous years of V4 data. This paper compares MODIS retrieved surface emissivities between V4, V4.1 and V5 using the level-3 MODIS daily LST&E product, MOD11B1.Comparisons of MOD11B1 retrieved surface emissivity during the Jul-Sep 2004 test period with lab measurements of sand samples collected at the Namib desert, Namibia result in a combined mean absolute emissivity difference for bands 29 (8.55 mu m), 31 (11 mu m) and 32 (12 mu m) of 1.06%, 0.65% and 1.93% for V4, V4.1 and V5 respectively. Maximum band 29 emissivity differences with the lab results were 4.10%, 2.96% and 8.64% for V4, V4.1 and V5 respectively. These results indicate that over and and semi-arid areas, users should consider using MODIS V4 or V4.1 data instead of V5. Furthermore, users should be careful not to develop time series from a mixture of product versions that could introduce artifacts at version boundaries. (C) 2009 Published by Elsevier Inc. C1 [Hulley, Glynn C.; Hook, Simon J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Hulley, GC (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM glynn.hulley@jpl.nasa.gov FU NASA Goddard Space Flight Center [M0D11B1] FX The research described in this paper was carried out at the jet Propulsion Laboratory, California Institute of Technology, under the contract with the National Aeronautics and Space Administration. We kindly thank Peter and Anne Hulley for providing the Namib dunes sand samples from Namibia. The geolocation code for the M0D11B1 tiles was provided by Dr. Zhengming Wan from the University of California Santa Barbara, and developed by Sadashiva Devadiga from NASA Goddard Space Flight Center. NR 14 TC 56 Z9 60 U1 0 U2 21 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 JUN 15 PY 2009 VL 113 IS 6 BP 1313 EP 1318 DI 10.1016/j.rse.2009.02.018 PG 6 WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic Technology SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science & Photographic Technology GA 446LP UT WOS:000266123400017 ER PT J AU Werdell, PJ Bailey, SW Franz, BA Harding, LW Feldman, GC McClain, CR AF Werdell, P. Jeremy Bailey, Sean W. Franz, Bryan A. Harding, Lawrence W., Jr. Feldman, Gene C. McClain, Charles R. TI Regional and seasonal variability of chlorophyll-a in Chesapeake Bay as observed by SeaWiFS and MODIS-Aqua SO REMOTE SENSING OF ENVIRONMENT LA English DT Article DE Chlorophyll; Remote sensing; Ocean color; Water quality; SeaWiFS; MODIS; Chesapeake Bay ID SATELLITE OCEAN COLOR; OPTICAL-PROPERTIES; ALGORITHM DEVELOPMENT; PRIMARY PRODUCTIVITY; MULTISENSOR APPROACH; ATLANTIC BIGHT; PHYTOPLANKTON; VALIDATION; RETRIEVAL; ESTUARIES AB Concentrations of the phytoplankton pigment chlorophyll-a (C-a) provide indicators of nutrient over-enrichment that has negatively affected Chesapeake Bay, U.S.A. C-a time-series from the National Aeronautics and Space Administration (NASA) Sea-viewing Wide Field-of-view Sensor (SeaWiFS) and Moderate Resolution Imaging Spectroradiometer aboard the Aqua spacecraft (MODIS-Aqua) provide observations on temporal and spatial scales that far exceed current field and aircraft sampling strategies. These sensors provide consistent, frequent, and high density data to potentially complement ongoing Bay monitoring activities. We used the in situ Water Quality Monitoring Data set of the Chesapeake Bay Program to evaluate decade-long time-series of SeaWiFS and MCDIS-Aqua C-a retrievals in the Bay. The accuracy of the retrievals generally degraded with increasing latitude as the optical complexity increases northward. C-a derived using empirical ("band ratio") algorithms overestimated in situ measurements by 10-50 and 40-100% for SeaWiFS and MODIS-Aqua, respectively, but with limited variability. C-a derived using spectral-matching algorithms showed less bias for both sensors, but with significant variability and sensitivity to radiometric errors. Regionally-tuned empirical algorithms performed best throughout the Bay, offering a combination of reasonable accuracy and high spatial coverage. The radiometric spectral resolution used as input to the algorithms strongly influenced the quality of C-a retrievals from both sensors. These results establish a baseline quantification of algorithm and sensor performance in a variable and stressed ecosystem against which novel approaches might be compared. (C) 2009 Elsevier Inc. All rights reserved. C1 [Werdell, P. Jeremy; Bailey, Sean W.; Franz, Bryan A.; Feldman, Gene C.; McClain, Charles R.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Harding, Lawrence W., Jr.] Univ Maryland, Ctr Environm Sci, Horn Point Lab, Cambridge, MD 21613 USA. RP Werdell, PJ (reprint author), Sci Syst & Applicat Inc, Lanham, MD 20706 USA. EM jeremy.werdell@nasa.gov RI Franz, Bryan/D-6284-2012; Werdell, Jeremy/D-8265-2012; Bailey, Sean/D-3077-2017 OI Franz, Bryan/0000-0003-0293-2082; Bailey, Sean/0000-0001-8339-9763 FU NASA MODIS Science Team FX We thank Michael Mallonee, David Jasinski, and Mark Trice for the assistance with the CBP Water Quality Monitoring data. We also thank Shawna Karlson, Kevin Sellner, Chris Kinkade, Eric Stengel, Michael Ondrusek, Chris Brown, and our anonymous reviewers for the valuable comments at various stages of this project. Support for this work was provided through the NASA MODIS Science Team. NR 49 TC 66 Z9 68 U1 1 U2 21 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 JUN 15 PY 2009 VL 113 IS 6 BP 1319 EP 1330 DI 10.1016/j.rse.2009.02.012 PG 12 WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic Technology SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science & Photographic Technology GA 446LP UT WOS:000266123400018 ER PT J AU Marzo, GA Roush, TL Lanza, NL McGuire, PC Newsom, HE Ollila, AM Wiseman, SM AF Marzo, G. A. Roush, T. L. Lanza, N. L. McGuire, P. C. Newsom, H. E. Ollila, A. M. Wiseman, S. M. TI Association of phyllosilicates and the inverted channel in Miyamoto crater, Mars SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID MERIDIANI-PLANUM; TERRA-MERIDIANI; STRATIGRAPHY; DEPOSITS; EXPRESS; HISTORY; ORIGIN AB The western floor of the Miyamoto crater in Sinus Meridiani on Mars exhibits both geomorphic and spectral evidence for aqueous history. It contains a sinuous and narrow ridge that is interpreted to be an inverted channel and is suggestive of past fluvial activity. Phyllosilicates occur in materials that are proximal to the paleochannel, but are not detected on top the ridge. The simultaneous use of the spectroscopic data, high-resolution images, and a digital elevation model show that Fe/Mg-smectites are exposed by erosion. They are associated with polygonally-fractured bedrock which occurs on the slopes of both sides of the sinuous ridge. The observations provide direct evidence of the presence of water and possibly of multiple aqueous events throughout the area. Citation: Marzo, G. A., T. L. Roush, N. L. Lanza, P. C. McGuire, H. E. Newsom, A. M. Ollila, and S. M. Wiseman (2009), Association of phyllosilicates and the inverted channel in Miyamoto crater, Mars, Geophys. Res. Lett., 36, L11204, doi:10.1029/2009GL038703. C1 [Marzo, G. A.; Roush, T. L.] NASA, Ames Res Ctr, Space Sci & Astrobiol Div, Moffett Field, CA 94035 USA. [Lanza, N. L.; Newsom, H. E.; Ollila, A. M.] Univ New Mexico, Inst Meteorit, Albuquerque, NM 87131 USA. [McGuire, P. C.] Free Univ Berlin, Inst Geosci, D-12249 Berlin, Germany. [Wiseman, S. M.] Washington Univ, Dept Earth & Planetary Sci, St Louis, MO 63130 USA. RP Marzo, GA (reprint author), NASA, Ames Res Ctr, Space Sci & Astrobiol Div, MS 245-3, Moffett Field, CA 94035 USA. EM giuseppe.marzo@nasa.gov RI McGuire, Patrick/D-2962-2013; Marzo, Giuseppe/A-9765-2015 OI McGuire, Patrick/0000-0001-6592-4966; FU NASA FX This research was supported by an appointment to the NASA Postdoctoral Program at the Ames Research Center, administered by Oak Ridge Associated Universities through a contract with NASA. TLR acknowledges NASA Mars Reconnaissance Orbiter Program for supporting his participation as a CRISM science team member. We are grateful to the CRISM, HiRISE, HRSC, MOLA, and THEMIS teams for making data available for this project. We wish to thank Alberto G. Fairen and an anonymous reviewer for helping us to improve the manuscript and Mark R. Salvatore for useful discussions. NR 24 TC 7 Z9 7 U1 0 U2 3 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 EI 1944-8007 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD JUN 13 PY 2009 VL 36 AR L11204 DI 10.1029/2009GL038703 PG 4 WC Geosciences, Multidisciplinary SC Geology GA 458FN UT WOS:000267000700008 ER PT J AU Miloshevich, LM Vomel, H Whiteman, DN Leblanc, T AF Miloshevich, Larry M. Voemel, Holger Whiteman, David N. Leblanc, Thierry TI Accuracy assessment and correction of Vaisala RS92 radiosonde water vapor measurements SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID DRY BIAS; HUMIDITY AB Relative humidity (RH) measurements from Vaisala RS92 radiosondes are widely used in research and operational applications, but their accuracy is not well characterized as a function of height, RH, and time of day (or solar altitude angle). This study compares RS92 RH measurements to simultaneous water vapor measurements from three reference instruments of known accuracy. Cryogenic frost point hygrometer measurements are used to characterize the RS92 accuracy above the 700-mbar level, microwave radiometer measurements characterize the RS92 accuracy averaged over essentially the lower troposphere, and the RS92 accuracy at the surface is characterized by a system of 6 RH probes with National Institute of Standards and Technology-traceable calibrations. The three RS92 accuracy assessments are combined to yield a detailed estimate of RS92 accuracy for all RH conditions from the surface to the lowermost stratosphere. An empirical correction is derived to remove the mean bias error, yielding corrected RS92 measurements whose bias uncertainty is independent of height or RH and is estimated to be +/- 4% of the measured RH value for nighttime soundings and +/- 5% for daytime soundings, plus an RH offset uncertainty of +/- 0.5% RH that is significant for dry conditions. The accuracy of an individual RS92 sounding is further characterized by the 1-sigma "random production variability,'' estimated to be +/- 1.5% of the measured RH value. The daytime bias correction must be used with caution, as it is only accurate for clear-sky or near-clear conditions owing to the complicated effect of clouds on the solar radiation error. C1 [Miloshevich, Larry M.] Natl Ctr Atmospher Res, Boulder, CO 80307 USA. [Leblanc, Thierry] NASA, Table Mt Observ, JPL, Pasadena, CA 91109 USA. [Voemel, Holger] Univ Colorado, CIRES, Boulder, CO 80309 USA. [Whiteman, David N.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Miloshevich, LM (reprint author), Natl Ctr Atmospher Res, POB 3000, Boulder, CO 80307 USA. EM milo@ucar.edu NR 10 TC 120 Z9 126 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 JUN 13 PY 2009 VL 114 AR D11305 DI 10.1029/2008JD011565 PG 23 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 458FZ UT WOS:000267002000002 ER PT J AU Driggers, WB Hoffmayer, ER AF Driggers, William B., III Hoffmayer, Eric R. TI Variability in the Reproductive Cycle of Finetooth Sharks, Carcharhinus isodon, in the Northern Gulf of Mexico SO COPEIA LA English DT Article ID ATLANTIC SHARPNOSE SHARK; RHIZOPRIONODON-TERRAENOVAE RICHARDSON; LIFE-HISTORY; BIOLOGY; ACRONOTUS; AGE AB From 2005 through 2008, seven mature female Finetooth Sharks, Carcharhinus isodon, were collected in the central northern Gulf of Mexico between April and June, a time coinciding with parturition and ovulation for the species. Five specimens displayed states of pregnancy and ovarian development consistent with a biennial reproductive cycle. Two individuals had near-term pups and vitellogenic oocytes, a condition Indicative of an annual reproductive cycle. These observations are the first report of annual reproduction In Finetooth Sharks and represent the first documented case of intraspecific divergence in the reproductive cycles for any elasmobranch within a discrete area. C1 [Driggers, William B., III] Natl Marine Fisheries Serv, SE Fisheries Sci Ctr, Mississippi Labs, Pascagoula, MS 39567 USA. [Hoffmayer, Eric R.] Univ So Mississippi, Ctr Fisheries Res & Dev, Gulf Coast Res Lab, Ocean Springs, MS 39564 USA. RP Driggers, WB (reprint author), Natl Marine Fisheries Serv, SE Fisheries Sci Ctr, Mississippi Labs, PO Drawer 1207, Pascagoula, MS 39567 USA. EM william.driggers@noaa.gov; eric.hoffmayer@usm.edu NR 12 TC 8 Z9 9 U1 0 U2 6 PU AMER SOC ICHTHYOLOGISTS HERPETOLOGISTS PI CHARLESTON PA UNIV CHARLESTON, GRICE MARINE LABORATORY, 205 FORT JOHNSON RD, CHARLESTON, SC 29412 USA SN 0045-8511 J9 COPEIA JI Copeia PD JUN 12 PY 2009 IS 2 BP 390 EP 393 DI 10.1643/CE-08-167 PG 4 WC Zoology SC Zoology GA 459YX UT WOS:000267151100023 ER PT J AU Sahraoui, F Goldstein, ML Robert, P Khotyaintsev, YV AF Sahraoui, F. Goldstein, M. L. Robert, P. Khotyaintsev, Yu. V. TI Evidence of a Cascade and Dissipation of Solar-Wind Turbulence at the Electron Gyroscale SO PHYSICAL REVIEW LETTERS LA English DT Article ID FIELD; DYNAMICS AB We report the first direct determination of the dissipation range of magnetofluid turbulence in the solar wind at the electron scales. Combining high resolution magnetic and electric field data of the Cluster spacecraft, we computed the spectrum of turbulence and found two distinct breakpoints in the magnetic spectrum at 0.4 and 35 Hz, which correspond, respectively, to the Doppler-shifted proton and electron gyroscales, f(rho p) and f(rho e). Below f(rho p), the spectrum follows a Kolmogorov scaling f(-1.62), typical of spectra observed at 1 AU. Above f(rho p), a second inertial range is formed with a scaling f(-2.3) down to f(rho e). Above f(rho e), the spectrum has a steeper power law similar to f(-4.1) down to the noise level of the instrument. We interpret this as the dissipation range and show a remarkable agreement with theoretical predictions of a quasi-two-dimensional cascade into Kinetic Alfveacuten Waves (KAW). C1 [Sahraoui, F.; Robert, P.] Ecole Polytech, CNRS, Lab Phys Plasmas, F-78140 Velizy Villacoublay, France. [Sahraoui, F.; Goldstein, M. L.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Khotyaintsev, Yu. V.] Swedish Inst Space Phys, Uppsala, Sweden. RP Sahraoui, F (reprint author), Ecole Polytech, CNRS, Lab Phys Plasmas, F-78140 Velizy Villacoublay, France. EM fouad.sahraoui@nasa.gov RI Khotyaintsev, Yuri/C-4745-2008; Goldstein, Melvyn/B-1724-2008 FU NASA/GSFC FX The FGM, PEACE, and CIS data come from the CAA (ESA) and AMDA (CESR, France). F. Sahraoui is funded partly by the NPP program at NASA/GSFC. NR 24 TC 299 Z9 299 U1 0 U2 10 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 JUN 12 PY 2009 VL 102 IS 23 AR 231102 DI 10.1103/PhysRevLett.102.231102 PG 4 WC Physics, Multidisciplinary SC Physics GA 457ZI UT WOS:000266977500012 PM 19658919 ER PT J AU Angelopoulos, V McFadden, JP Larson, D Carlson, CW Mende, SB Frey, H Phan, T Sibeck, DG Glassmeier, KH Auster, U Donovan, E Mann, IR Rae, IJ Russell, CT Runov, A Zhou, XZ Kepko, L AF Angelopoulos, Vassilis McFadden, James P. Larson, Davin Carlson, Charles W. Mende, Stephen B. Frey, Harald Phan, Tai Sibeck, David G. Glassmeier, Karl-Heinz Auster, Uli Donovan, Eric Mann, Ian R. Rae, I. Jonathan Russell, Christopher T. Runov, Andrei Zhou, Xu-Zhi Kepko, Larry TI Response to Comment on "Tail Reconnection Triggering Substorm Onset" SO SCIENCE LA English DT Editorial Material ID MAGNETIC RECONNECTION; MAGNETOTAIL AB Lui challenges our conclusion that magnetic reconnection triggered the onset of a magnetospheric substorm. However, Lui incorrectly uses the auroral electrojet index instead of ground auroral and magnetic field pulsation signatures to determine substorm onset; single velocity and magnetic field components instead of full vectors and particle distributions to identify reconnection onset; and preliminary auroral electrojet-low index (AL) instead of ground magnometer, auroral, and magnetotail data to claim pre-existing activity. C1 [Angelopoulos, Vassilis; Russell, Christopher T.; Runov, Andrei; Zhou, Xu-Zhi] Univ Calif Los Angeles, Dept Earth & Space Sci, Inst Geophys & Planetary Phys, Los Angeles, CA 90095 USA. [McFadden, James P.; Larson, Davin; Carlson, Charles W.; Mende, Stephen B.; Frey, Harald; Phan, Tai] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94729 USA. [Sibeck, David G.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Glassmeier, Karl-Heinz; Auster, Uli] Tech Univ Carolo Wilhelmina Braunschweig, D-38106 Braunschweig, Germany. [Donovan, Eric] Univ Calgary, Dept Phys & Astron, Calgary, AB T2N 1N4, Canada. [Mann, Ian R.; Rae, I. Jonathan] Univ Alberta, Dept Phys, Edmonton, AB T6G 2M7, Canada. [Kepko, Larry] Univ New Hampshire, Ctr Space Sci, Durham, NH 03824 USA. RP Angelopoulos, V (reprint author), Univ Calif Los Angeles, Dept Earth & Space Sci, Inst Geophys & Planetary Phys, Los Angeles, CA 90095 USA. EM vassilis@ucla.edu RI Zhou, Xuzhi/D-1831-2011; Sibeck, David/D-4424-2012; Kepko, Larry/D-7747-2012; Rae, Jonathan/D-8132-2013; OI Zhou, Xuzhi/0000-0003-4953-1761; Kepko, Larry/0000-0002-4911-8208; Donovan, Eric/0000-0002-8557-4155; Frey, Harald/0000-0001-8955-3282 NR 7 TC 40 Z9 40 U1 0 U2 5 PU AMER ASSOC ADVANCEMENT SCIENCE PI WASHINGTON PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 USA SN 0036-8075 J9 SCIENCE JI Science PD JUN 12 PY 2009 VL 324 IS 5933 DI 10.1126/science.1168045 PG 3 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 456VD UT WOS:000266878700024 ER PT J AU Saether, E Yamakov, V Glaessgen, EH AF Saether, E. Yamakov, V. Glaessgen, E. H. TI An embedded statistical method for coupling molecular dynamics and finite element analyses SO INTERNATIONAL JOURNAL FOR NUMERICAL METHODS IN ENGINEERING LA English DT Article DE multiscale analysis; molecular dynamics; finite element methods ID DISLOCATION NUCLEATION; ATOMISTIC SIMULATIONS; BOUNDARY-CONDITIONS; BRIDGING DOMAIN; LENGTH SCALES; CONTINUUM; SOLIDS; TEMPERATURE; FRACTURE; ALUMINUM AB The coupling of molecular dynamics (MD) simulations with finite element methods (FEM) yields computationally efficient models that link fundamental material processes at the atomistic level with continuum field responses at higher length scales. The theoretical challenge involves developing a seamless connection along an interface between two inherently different simulation frameworks. Various specialized methods have been developed to solve particular classes of problems. Many of these methods link the kinematics of individual MID atoms with finite element (FE) nodes at their common interface, necessarily requiring that the FE mesh be refined to atomic resolution. Some of these coupling approaches also require simulations to be carried out at OK and restrict modelling to two-dimensional material domains due to difficulties in simulating full three-dimensional material processes. In the present work, a new approach to MD-FEM coupling is developed based oil a restatement of the standard boundary value problem used to define a coupled domain. The method replaces a direct linkage of individual MID atoms and FE nodes with a statistical averaging of atomistic displacements in local atomic volumes associated with each FE node in an interface region. The FEM and MID computational systems are effectively independent and communicate only through an iterative update of their boundary conditions. Thus, the method lends itself for use with any FEM or MID code. With the use of statistical averages of the atomistic quantities to Couple the two computational schemes, the developed approach is referred to as an embedded statistical coupling method (ESCM). ESCM provides an enhanced coupling methodology that is inherently applicable to three-dimensional domains, avoids discretization of the continuum model to atomic scale resolution, and permits finite temperature states to be applied. Published in 2009 by John Wiley & Sons, Ltd. C1 [Saether, E.; Glaessgen, E. H.] NASA, Langley Res Ctr, Hampton, VA 23681 USA. [Yamakov, V.] Natl Inst Aerosp, Hampton, VA 23666 USA. RP Saether, E (reprint author), NASA, Langley Res Ctr, Hampton, VA 23681 USA. EM erik.saether-1@nasa.gov NR 41 TC 23 Z9 24 U1 0 U2 25 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0029-5981 J9 INT J NUMER METH ENG JI Int. J. Numer. Methods Eng. PD JUN 11 PY 2009 VL 78 IS 11 BP 1292 EP 1319 DI 10.1002/nme.2529 PG 28 WC Engineering, Multidisciplinary; Mathematics, Interdisciplinary Applications SC Engineering; Mathematics GA 459VM UT WOS:000267139900002 ER PT J AU Rietmeijer, FJM Pun, A Nuth, JA AF Rietmeijer, Frans J. M. Pun, Aurora Nuth, Joseph A., III TI Dust formation and evolution in a Ca-Fe-SiO-H-2-O-2 vapour phase condensation experiment and astronomical implications SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE astrochemistry; methods: laboratory; Solar system: general; planetary systems: protoplanetary discs ID METASTABLE EUTECTIC CONDENSATION; CIRCUMSTELLAR DUST; SOLID CONDENSATION; LIGHT-SCATTERING; SILICATE SMOKES; COSMIC DUST; ANALOGS; GRAINS; SYSTEM; GAS AB Here, we report on a kinetically controlled vapour phase condensation experiment using a low-calcium Ca-Fe-SiO-H-2-O-2 vapour. Under these conditions of extreme disequilibrium, the condensate properties become predictable. They are amorphous solids with (predictable) deep metastable eutectic compositions. This study also shows how chemical evolution of the condensate grains will lead to chemically complex amorphous solids. The highly disordered structure of the deep metastable eutectic condensates is the very key to this predictable chemical evolution to grains with a silicate mineral composition, yet being amorphous. We compare our results with astronomical observations of dust around young stellar objects. C1 [Rietmeijer, Frans J. M.; Pun, Aurora] 1 Univ New Mexico, Dept Earth & Planetary Sci, Albuquerque, NM 87131 USA. [Nuth, Joseph A., III] NASA, Goddard Space Flight Ctr, Solar Syst Explorat Div, Astrochem Lab, Greenbelt, MD 20771 USA. RP Rietmeijer, FJM (reprint author), 1 Univ New Mexico, Dept Earth & Planetary Sci, MSC03-2040, Albuquerque, NM 87131 USA. EM fransjmr@unm.edu RI Nuth, Joseph/E-7085-2012 FU NASA [NNG04GM48A, NNX07AI39G] FX We are grateful for a constructive review. FJMR and AP acknowledge the support from NASA grants NNG04GM48A and NNX07AI39G. JAN is grateful for support from the Cosmochemistry Program at NASA Headquarters. Samples were produced in the Astrochemistry Laboratory of the NASA Goddard Space Flight Center. The HRTEM analyses were performed in the Electron Microbeam Analyses Facility of the Department of Earth and Planetary Sciences at UNM. NR 40 TC 5 Z9 5 U1 0 U2 0 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 JUN 11 PY 2009 VL 396 IS 1 BP 402 EP 408 DI 10.1111/j.1365-2966.2009.14703.x PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 453KT UT WOS:000266610000050 ER PT J AU Samal, PK Saha, R Jain, P Ralston, JP AF Samal, Pramoda Kumar Saha, Rajib Jain, Pankaj Ralston, John P. TI Signals of statistical anisotropy in WMAP foreground-cleaned maps SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE methods: data analysis; cosmic microwave background; cosmology: miscellaneous ID MICROWAVE BACKGROUND ANOMALIES; POWER-SPECTRUM; RADIO POLARIZATIONS; COSMOLOGICAL SCALES; SKY; ASYMMETRY; ISOTROPY; PROPAGATION; MULTIPOLES; RADIATION AB Recently, a symmetry-based method to test for statistical isotropy of the cosmic microwave background was developed. We apply the method to template-cleaned 3- and 5-years Wilkinson Microwave Anisotropy Probe-Differencing Assembly maps. We examine a wide range of angular multipoles from 2 < l < 300. The analysis detects statistically significant signals of anisotropy inconsistent with an isotropic cosmic microwave background in some of the foreground-cleaned maps. We are unable to resolve whether the anomalies have a cosmological, local astrophysical or instrumental origin. Assuming the anisotropy arises due to residual foreground contamination, we estimate the residual foreground power in the maps. For the W-band maps, we also find a highly improbable degree of isotropy we cannot explain. We speculate that excess isotropy may be caused by faulty modelling of detector noise. C1 [Samal, Pramoda Kumar; Jain, Pankaj] Indian Inst Technol, Dept Phys, Kanpur 208016, Uttar Pradesh, India. [Saha, Rajib] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Saha, Rajib] CALTECH, Pasadena, CA 91125 USA. [Ralston, John P.] Univ Kansas, Dept Phys & Astron, Lawrence, KS 66045 USA. RP Samal, PK (reprint author), Indian Inst Technol, Dept Phys, Kanpur 208016, Uttar Pradesh, India. EM samal@iitk.ac.in; Rajib.Saha@jpl.nasa.gov; pkjain@iitk.ac.in; ralston@ku.edu FU CSIR, India [CSIR-SRF-9/92(340)/2004-EMR-I]; DOE [DE-FG02-04ER14308]; National Aeronautics and Space Administration FX We acknowledge the use of Legacy Archive for Microwave Background Data Analysis. Some of the results of this work are derived using the publicly available HEALPIX package (Gorski et al. 2005). PKS acknowledges CSIR, India for financial support under the research grant CSIR-SRF-9/92(340)/2004-EMR-I. JPR is supported in part under DOE Grant Number DE-FG02-04ER14308. A portion of the research described in this paper was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. NR 79 TC 30 Z9 30 U1 0 U2 0 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD JUN 11 PY 2009 VL 396 IS 1 BP 511 EP 522 DI 10.1111/j.1365-2966.2009.14728.x PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 453KT UT WOS:000266610000057 ER PT J AU Schnabel, KE Martin, JW Moffitt, RB AF Schnabel, Kareen E. Martin, Joel W. Moffitt, Robert B. TI Additions to the decapod crustacean fauna of the Hawaiian Islands, III. A new species of the genus Babamunida (Crustacea: Galatheidae) from Hawaii based on morphological and molecular evidence SO ZOOTAXA LA English DT Article DE Anomura; squat lobster; DNA; 16S; CO1; taxonomy; central Pacific; ROV; Hawaii ID SOUTH-WEST PACIFIC AB Babamunida kanaloa n. sp., a new galatheid from approximately 250 m depth off the Northwestern Hawaiian Islands (French Frigate Shoals), is described. DNA sequence data from two gene regions (16S and CO1) corroborates the placement of this new species in the genus Babamunida. Images taken independently using the Deep Submergence Vehicle Pisces IV are almost certainly of the same species based on overall size and color pattern and provide limited ecological information. This new species brings the number of species in the genus Babamunida to six and the total number of galatheid species known from the Hawaiian Islands to four (possibly higher depending on some previous records that might be questionable). C1 [Schnabel, Kareen E.] Natl Inst Water & Atmospher Res, Wellington, New Zealand. [Martin, Joel W.] Nat Hist Museum Angeles Cty, Los Angeles, CA 90007 USA. [Moffitt, Robert B.] NOAA, Natl Marine Fisheries Serv, SW Fisheries Sci Ctr, Honolulu Lab, Honolulu, HI 96822 USA. RP Schnabel, KE (reprint author), Natl Inst Water & Atmospher Res, Private Bag 14901, Wellington, New Zealand. EM k.schnabel@niwa.co.nz; jmartin@nhm.org; Robert.Moffitt@noaa.gov FU National Science Foundation's [DEB 0531616]; Darryl Felder (University of Louisiana Lafayette); Rodney Feldmann; Kent State University FX This work was supported in part by grant number DEB 0531616 from the National Science Foundation's "Assembling the Tree of Life" program to J. W. Martin, in conjunction with collaborative awards to Keith Crandall and Nikki Hannegan (Brigham Young University), Darryl Felder (University of Louisiana Lafayette), and Rodney Feldmann and Carrie Schweitzer (Kent State University). NR 14 TC 13 Z9 13 U1 0 U2 0 PU MAGNOLIA PRESS PI AUCKLAND PA PO BOX 41383, AUCKLAND, ST LUKES 1030, NEW ZEALAND SN 1175-5326 EI 1175-5334 J9 ZOOTAXA JI Zootaxa PD JUN 11 PY 2009 IS 2130 BP 21 EP 30 PG 10 WC Zoology SC Zoology GA 457CC UT WOS:000266902000002 ER PT J AU Currie, T Lada, CJ Plavchan, P Robitaille, TP Irwin, J Kenyon, SJ AF Currie, Thayne Lada, Charles J. Plavchan, Peter Robitaille, Thomas P. Irwin, Jonathan Kenyon, Scott J. TI THE LAST GASP OF GAS GIANT PLANET FORMATION: A SPITZER STUDY OF THE 5 Myr OLD CLUSTER NGC 2362 SO ASTROPHYSICAL JOURNAL LA English DT Article DE circumstellar matter; open clusters and associations (individual: NGC 2362); planetary systems: formation; planetary systems: protoplanetary disks; stars: pre-main sequence ID LOW-MASS STARS; YOUNG STELLAR OBJECTS; T-TAURI STARS; SPECTRAL ENERGY-DISTRIBUTIONS; DEBRIS DISK CANDIDATES; INFRARED ARRAY CAMERA; MAIN-SEQUENCE STARS; CIRCUMSTELLAR DISK; SPACE-TELESCOPE; CHI-PERSEI AB Expanding upon the Infrared Array Camera (IRAC) survey from Dahm & Hillenbrand, we describe Spitzer IRAC and Multiband Imaging Photometer for Spitzer observations of the populous, 5 Myr old open cluster NGC 2362. We analyze the mid-IR colors of cluster members and compared their spectral energy distributions (SEDs) to star+circumstellar disk models to constrain the disk morphologies and evolutionary states. Early/intermediate-type confirmed/candidate cluster members either have photospheric mid-IR emission or weak, optically thin IR excess emission at lambda >= 24 mu m consistent with debris disks. Few late-type, solar/subsolar-mass stars have primordial disks. The disk population around late-type stars is dominated by disks with inner holes (canonical "transition disks") and "homologously depleted" disks. Both types of disks represent an intermediate stage between primordial disks and debris disks. Thus, in agreement with previous results, we find that multiple paths for the primordial-to-debris disk transition exist. Because these "evolved primordial disks" greatly outnumber primordial disks, our results undermine standard arguments in favor of a less than or similar to 10(5) yr timescale for the transition based on data from Taurus-Auriga. Because the typical transition timescale is far longer than 10(5) yr, these data also appear to rule out standard ultraviolet photoevaporation scenarios as the primary mechanism to explain the transition. Combining our data with other Spitzer surveys, we investigate the evolution of debris disks around high/intermediate-mass stars and investigate timescales for giant planet formation. Consistent with Currie et al., the luminosity of 24 mu m emission in debris disks due to planet formation peaks at approximate to 10-20 Myr. If the gas and dust in disks evolve on similar timescales, the formation timescale for gas giant planets surrounding early-type, high/intermediate-mass (greater than or similar to 1.4 M-circle dot) stars is likely 1-5 Myr. Most solar/subsolar-mass stars detected by Spitzer have SEDs that indicate their disks may be actively leaving the primordial disk phase. Thus, gas giant planet formation may also occur by similar to 5 Myr around solar/subsolar-mass stars as well. C1 [Currie, Thayne; Lada, Charles J.; Robitaille, Thomas P.; Irwin, Jonathan; Kenyon, Scott J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02140 USA. [Plavchan, Peter] CALTECH, NASA, Exoplanet Sci Inst, Pasadena, CA 91125 USA. [Irwin, Jonathan] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. RP Currie, T (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02140 USA. EM tcurrie@cfa.harvard.edu; clada@cfa.harvard.edu; plavchan@ipac.caltech.edu; trobitaille@cfa.harvard.edu; jirwin@cfa.harvard.edu; skenyon@cfa.harvard.edu OI Kenyon, Scott/0000-0003-0214-609X; Robitaille, Thomas/0000-0002-8642-1329 FU NASA through the Spitzer Space Telescope Fellowship Program (TPR) FX We thank Richard Alexander for useful comments about UV photoevaporation and Adam Kraus for very informative discussions on the role of binarity in disk evolution. We also thank Carol Grady for pointing out constraints on the formation of Saturn from the planetary science community. Support for this work was provided by NASA through the Spitzer Space Telescope Fellowship Program (TPR). NR 90 TC 103 Z9 103 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 JUN 10 PY 2009 VL 698 IS 1 BP 1 EP 27 DI 10.1088/0004-637X/698/1/1 PG 27 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 450AP UT WOS:000266373700001 ER PT J AU Racusin, JL Liang, EW Burrows, DN Falcone, A Sakamoto, T Zhang, BB Zhang, B Evans, P Osborne, J AF Racusin, J. L. Liang, E. W. Burrows, D. N. Falcone, A. Sakamoto, T. Zhang, B. B. Zhang, B. Evans, P. Osborne, J. TI JET BREAKS AND ENERGETICS OF Swift GAMMA-RAY BURST X-RAY AFTERGLOWS SO ASTROPHYSICAL JOURNAL LA English DT Review DE gamma rays: bursts; radiation mechanisms: non-thermal; X-rays: bursts ID CONTINUOUS ENERGY INJECTION; LIGHT-CURVES; XRT DATA; COMPREHENSIVE ANALYSIS; SPECTRAL EVOLUTION; HOST GALAXY; GRB AFTERGLOWS; 1ST SURVEY; EMISSION; PROMPT AB We present a systematic temporal and spectral study of all Swift-X-ray Telescope observations of gamma-ray burst (GRB) afterglows discovered between 2005 January and 2007 December. After constructing and fitting all light curves and spectra to power-law models, we classify the components of each afterglow in terms of the canonical X-ray afterglow and test them against the closure relations of the forward shock models for a variety of parameter combinations. The closure relations are used to identify potential jet breaks with characteristics including the uniform jet model with and without lateral spreading and energy injection, and a power-law structured jet model, all with a range of parameters. With this technique, we survey the X-ray afterglows with strong evidence for jet breaks (similar to 12% of our sample), and reveal cases of potential jet breaks that do not appear plainly from the light curve alone (another similar to 30%), leading to insight into the missing jet break problem. Those Xray light curves that do not show breaks or have breaks that are not consistent with one of the jet models are explored to place limits on the times of unseen jet breaks. The distribution of jet break times ranges from a few hours to a few weeks with a median of similar to 1 day, similar to what was found pre-Swift. On average, Swift GRBs have lower isotropic equivalent gamma-ray energies, which in turn result in lower collimation corrected gamma-ray energies than those of pre-Swift GRBs. Finally, we explore the implications for GRB jet geometry and energetics. C1 [Racusin, J. L.; Burrows, D. N.; Falcone, A.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Liang, E. W.; Zhang, B. B.; Zhang, B.] Univ Nevada, Dept Phys, Las Vegas, NV 89154 USA. [Liang, E. W.] Guangxi Univ, Dept Phys, Nanning 530004, Peoples R China. [Sakamoto, T.] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA. [Evans, P.; Osborne, J.] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England. RP Racusin, JL (reprint author), Penn State Univ, Dept Astron & Astrophys, 525 Davey Lab, University Pk, PA 16802 USA. EM racusin@astro.psu.edu RI Racusin, Judith/D-2935-2012; Zhang, Binbin/C-9035-2013 OI Zhang, Binbin/0000-0003-2002-116X FU NASA [NAS5-00136, NNG05GB67G, NNX08AN24G, NNX08AE57A]; UNLV; National Natural Science Foundation of China [10873002]; National Basic Research Program ("973" Program) of China [2009CB824800]; foundation of Guangxi University FX J.L.R., D.N.B., and A. F. gratefully acknowledge support for this work from NASA contract NAS5-00136. We acknowledge the use of public data from the Swift data archive. B.Z.,B. B.Z, and E.-W.L. gratefully acknowledge support from NASA contracts NNG05GB67G, NNX08AN24G, NNX08AE57A, and a President's Infrastructure Award from UNLV. E.-W.L. also acknowledges support from a National Natural Science Foundation of China grant 10873002, National Basic Research Program ("973" Program) of China (grant 2009CB824800), and the research foundation of Guangxi University. This work made use of data supplied by the UK Swift Science Data Centre at the University of Leicester. We thank R. Willingale for his helpful comments. NR 178 TC 135 Z9 136 U1 0 U2 6 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JUN 10 PY 2009 VL 698 IS 1 BP 43 EP 74 DI 10.1088/0004-637X/698/1/43 PG 32 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 450AP UT WOS:000266373700003 ER PT J AU Turner, TJ Miller, L Kraemer, SB Reeves, JN Pounds, KA AF Turner, T. J. Miller, L. Kraemer, S. B. Reeves, J. N. Pounds, K. A. TI SUZAKU OBSERVATION OF A HARD EXCESS IN 1H 0419-577: DETECTION OF A COMPTON-THICK PARTIAL-COVERING ABSORBER SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: active; galaxies: individual (1H 0419-577); galaxies: Seyfert; X-rays: galaxies ID ACTIVE GALACTIC NUCLEI; X-RAY-SPECTRUM; BROAD-LINE REGION; KERR BLACK-HOLE; SEYFERT-GALAXIES; XMM-NEWTON; ABSORPTION LINES; QUASAR PDS-456; COLD MATTER; IRON LINE AB We present results from a 200 ks Suzaku observation of 1H 0419-577 taken during 2007 July. The source shows a strong excess of counts above 10 keV compared to the extrapolation of models based on previous data in the 0.5-10 keV band. The "hard excess" in 1H 0419-577 can be explained by the presence of a Compton-thick partial-covering absorber that covers similar to 70% of the source. The Compton-thick gas likely originates from a radius inside of the optical broad-line region and may form part of a clumpy disk wind. The fluorescent Fe K alpha luminosity measured by Suzaku is consistent with that expected from an equatorial disk wind. C1 [Turner, T. J.] Univ Maryland Baltimore Cty, Dept Phys, Baltimore, MD 21250 USA. [Turner, T. J.; Kraemer, S. B.] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA. [Miller, L.] Univ Oxford, Dept Phys, Oxford OX1 3RH, England. [Kraemer, S. B.] Catholic Univ Amer, Dept Phys, Inst Astrophys & Computat Sci, Washington, DC 20064 USA. [Reeves, J. N.] Univ Keele, Sch Phys & Geog Sci, Astrophys Grp, Keele ST5 5BG, Staffs, England. [Pounds, K. A.] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England. RP Turner, TJ (reprint author), Univ Maryland Baltimore Cty, Dept Phys, Baltimore, MD 21250 USA. RI XRAY, SUZAKU/A-1808-2009 FU NASA [NNX08AL50G, NAS5-26555, NAG5-7584]; STFC [PP/E001114/1] FX T.J.T. acknowledges NASA grant NNX08AL50G. L. M. acknowledges STFC grant number PP/E001114/1. We thank the anonymous referee for comments that helped improve this manuscript. We are also grateful to the Suzaku operations team for performing this observation and providing software and calibration for the data analysis. Some of the data presented in this paper were obtained from the Multi-mission Archive at the Space Telescope Science Institute (MAST). STScI is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS5-26555. Support for MAST for non-HST data is provided by the NASA Office of Space Science via grant NAG5-7584 and by other grants and contracts. This research has also made use of data obtained from the High Energy Astrophysics Science Archive Research Center (HEASARC), provided by NASA's Goddard Space Flight Center. NR 65 TC 43 Z9 43 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 JUN 10 PY 2009 VL 698 IS 1 BP 99 EP 105 DI 10.1088/0004-637X/698/1/99 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 450AP UT WOS:000266373700006 ER PT J AU Kraemer, SB Trippe, ML Crenshaw, DM Melendez, M Schmitt, HR Fischer, TC AF Kraemer, S. B. Trippe, M. L. Crenshaw, D. M. Melendez, M. Schmitt, H. R. Fischer, T. C. TI PHYSICAL CONDITIONS IN THE INNER NARROW-LINE REGION OF THE SEYFERT 2 GALAXY MARKARIAN 573 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: active; galaxies: individual (Mrk 573); galaxies: Seyfert ID ACTIVE GALACTIC NUCLEI; PRESSURE-DOMINATED PHOTOIONIZATION; HUBBLE-SPACE-TELESCOPE; RESOLVED SPECTROSCOPY; INTRINSIC ABSORPTION; ULTRAVIOLET-SPECTRA; HOST GALAXIES; EXTENDED GAS; BLACK-HOLE; MU-M AB We have examined the physical conditions within a bright emission-line knot in the inner narrow-line region (NLR) of the Seyfert 2 galaxy Mrk 573 using optical spectra and photoionization models. The spectra were obtained with the Hubble Space Telescope/Space Telescope Imaging Spectrograph, through the 0 ''.2 x 52 ''.0 slit, at a position angle of -71 degrees.2, with the G430L and G750M gratings. Comparing the spatial emission-line profiles, we found [Fe x]. 6734 barely resolved, [O III] lambda 5007 centrally peaked, but broader than [Fe X], and [O II] lambda 3727 the most extended. Spectra of the central knot were extracted from a region 1 ''.1 in extent, corresponding to the full width at zero intensity in the cross-dispersion direction, of the knot. The spectra reveal that [Fe X] is broader in velocity width and blueshifted compared with lines from less ionized species. Our estimate of the bolometric luminosity indicates that the active galactic nucleus (AGN) is radiating at or above its Eddington luminosity, which is consistent with its identification as a hidden Narrow-Line Seyfert 1. We were able to successfully match the observed emission-line ratios with a three-component photoionization model. Two components, one to account for the [O III] emission and another in which the [Fe X] arises, are directly ionized by the AGN, while [O II] forms in a third component, which is ionized by a heavily absorbed continuum. Based on our assumed ionizing continuum and the model parameters, we determined that the two directly ionized components are similar to 55 pc from the AGN. We have found similar radial distances for the central knots in the Seyfert 2 galaxies Mrk 3 and NGC 1068, but much smaller radial distances for the inner NLR in the Seyfert 1 galaxies NGC 4151 and NGC 5548. Although in general agreement with the unified model, these results suggest that the obscuring material in Seyfert galaxies extends out to at least tens of parsecs from the AGN. C1 [Kraemer, S. B.] Catholic Univ Amer, Dept Phys, Inst Astrophys & Computat Sci, Washington, DC 20064 USA. [Kraemer, S. B.] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA. [Trippe, M. L.; Crenshaw, D. M.; Fischer, T. C.] Georgia State Univ, Dept Phys & Astron, Astron Off, Atlanta, GA 30303 USA. [Schmitt, H. R.] USN, Res Lab, Remote Sensing Div, Washington, DC 20375 USA. [Schmitt, H. R.] Interferometrics Inc, Herndon, VA 20171 USA. RP Kraemer, SB (reprint author), Catholic Univ Amer, Dept Phys, Inst Astrophys & Computat Sci, Washington, DC 20064 USA. FU NASA [NAS5-26555]; Office of Naval Research; 6.1 base funding FX This research made use of the NASA/IPAC Extragalactic Database (NED), which is operated by the Jet Propulsion Laboratory, Caltech, under contract with NASA. The observations used in this paper were obtained with the NASA/ESA Hubble Space Telescope at the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS5-26555. Basic research at the US Naval Research Laboratory (NRL) is supported by the Office of Naval Research. Basic research in astronomy at NRL is supported by 6.1 base funding. We thank Gary Ferland for his continued development and maintenance of CLOUDY. We thank the referee, Hagai Netzer, for helpful and insightful comments. NR 68 TC 20 Z9 20 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 JUN 10 PY 2009 VL 698 IS 1 BP 106 EP 114 DI 10.1088/0004-637X/698/1/106 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 450AP UT WOS:000266373700007 ER PT J AU Bauschlicher, CW Ricca, A AF Bauschlicher, Charles W., Jr. Ricca, Alessandra TI THE FAR-INFRARED EMISSION FROM THE Mg+-PAH SPECIES SO ASTROPHYSICAL JOURNAL LA English DT Article DE astrochemistry; infrared: ISM; ISM: molecules; methods: numerical ID POLYCYCLIC AROMATIC-HYDROCARBONS; GAUSSIAN-BASIS SETS; ELECTRON CORRELATION; ISO SPECTROSCOPY; LARGE MOLECULES; SPECTRA; DUST; GALAXIES; CATIONS; BANDS AB The far-infrared (FIR) spectra of several Mg+-PAH species are studied using density functional theory. The Mg+-PAH stretching mode, regardless of the polycyclic aromatic hydrocarbon (PAH) species, carries a reasonable intensity and tends to fall in a narrow range near 40 mu m. Because the bands tend to fall at very similar frequencies, the average spectra of several Mg+-PAH species produce a broadband with an intensity that is about 20% of the well known C-H out-of-plane bending mode. In contrast, an average of seven large compact pure PAHs has no FIR bands that carry any significant intensity. C1 [Ricca, Alessandra] SETI Inst, Carl Sagan Ctr, Mountain View, CA 94043 USA. [Bauschlicher, Charles W., Jr.; Ricca, Alessandra] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Bauschlicher, CW (reprint author), Space Technol Div, Mail Stop 230-3, Moffett Field, CA 94035 USA. EM Charles.W.Bauschlicher@nasa.gov; Alessandra.Ricca-1@nasa.gov FU NASA's Astronomy and Physics Research and Analysis (APRA) [NNX07AH02G]; Astrophysics Theory, Fundamental Physics (ATFP) [NNX09AD18G]; Astrophysics Data Analysis Program (ADP) [NNX09AD84G] FX These authors thank Andy Mattioda and Lou Allamandola for helpful discussions. We acknowledge financial support form NASA's Astronomy and Physics Research and Analysis (APRA) (grant NNX07AH02G), Astrophysics Theory, Fundamental Physics (ATFP) (grant NNX09AD18G), and Astrophysics Data Analysis Program (ADP) (grant NNX09AD84G). NR 35 TC 10 Z9 10 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JUN 10 PY 2009 VL 698 IS 1 BP 275 EP 280 DI 10.1088/0004-637X/698/1/275 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 450AP UT WOS:000266373700021 ER PT J AU Kaltenegger, L Traub, WA AF Kaltenegger, Lisa Traub, Wesley A. TI TRANSITS OF EARTH-LIKE PLANETS SO ASTROPHYSICAL JOURNAL LA English DT Article DE astrobiology; Earth; planets and satellites: general; techniques: spectroscopic ID EXTRA-SOLAR PLANETS; M-CIRCLE-PLUS; MOLECULAR SPECTROSCOPIC DATABASE; HARPS SEARCH; SUPER-EARTH; HD 189733B; M-DWARFS; TERRESTRIAL PLANETS; THERMAL EMISSION; NEARBY-STAR AB Transmission spectroscopy of Earth-like exoplanets is a potential tool for habitability screening. Transiting planets are present-day "Rosetta Stones" for understanding extrasolar planets because they offer the possibility to characterize giant planet atmospheres and should provide an access to biomarkers in the atmospheres of Earth-like exoplanets, once they are detected. Using the Earth itself as a proxy we show the potential and limits of the transiting technique to detect biomarkers on an Earth-analog exoplanet in transit. We quantify the Earth's cross section as a function of wavelength, and show the effect of each atmospheric species, aerosol, and Rayleigh scattering. Clouds do not significantly affect this picture because the opacity of the lower atmosphere from aerosol and Rayleigh losses dominates over cloud losses. We calculate the optimum signal-to-noise ratio for spectral features in the primary eclipse spectrum of an Earth-like exoplanet around a Sun-like star and also M stars, for a 6.5 m telescope in space. We find that the signal-to-noise values for all important spectral features are on the order of unity or less per transit-except for the closest stars-making it difficult to detect such features in one single transit, and implying that coadding of many transits will be essential. C1 [Kaltenegger, Lisa; Traub, Wesley A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Traub, Wesley A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Kaltenegger, L (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM lkaltenegger@cfa.harvard.edu FU NASA [NAG5-13045] FX We are grateful to Neill Reid for providing us with the M-star data and Todd Henry for providing us with a list of the closest M stars. Special thanks to Ken Jucks, Sara Seager, and Phillip Nutzman for stimulating discussion and comments. This work was sponsored by NASA grant NAG5-13045 at the Harvard Smithsonian Center for Astrophysics and the Origins of Life Initiative at Harvard. Part of the research described in this paper was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. NR 47 TC 116 Z9 116 U1 2 U2 24 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 JUN 10 PY 2009 VL 698 IS 1 BP 519 EP 527 DI 10.1088/0004-637X/698/1/519 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 450AP UT WOS:000266373700042 ER PT J AU Brenneman, LW Weaver, KA Kadler, M Tueller, J Marscher, A Ros, E Zensus, A Kovalev, YY Aller, M Aller, H Irwin, J Kerp, J Kaufmann, S AF Brenneman, L. W. Weaver, K. A. Kadler, M. Tueller, J. Marscher, A. Ros, E. Zensus, A. Kovalev, Y. Y. Aller, M. Aller, H. Irwin, J. Kerp, J. Kaufmann, S. TI SPECTRAL ANALYSIS OF THE ACCRETION FLOW IN NGC 1052 WITH SUZAKU SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; galaxies: active; galaxies: individual (NGC 1052); X-rays: individual (NGC 1052) ID DISK-JET CONNECTION; X-RAY VARIABILITY; K-ALPHA LINE; BLACK-HOLE; SEYFERT-GALAXIES; GALACTIC NUCLEI; RADIO; EMISSION; ORIGIN; NGC-1052 AB We present an analysis of the 101 ks, 2007 Suzaku spectrum of the low ionization nuclear emission region galaxy NGC 1052. The 0.5-10 keV continuum is well modeled by a power-law continuum modified by Galactic and intrinsic absorption, and it exhibits a soft, thermal emission component below 1 keV. Both a narrow core and a broader component of Fe Ka emission centered at 6.4 keV are robustly detected. While the narrow line is consistent with an origin in material distant from the black hole, the broad line is best fit empirically by a model that describes fluorescent emission from the inner accretion disk around a rapidly rotating black hole. We find no evidence in this observation for Comptonized reflection of the hard X-ray source by the disk above 10 keV, however, which casts doubt on the hypothesis that the broad iron line originates in the inner regions of a standard accretion disk. We explore other possible scenarios for producing this spectral feature and conclude that the high equivalent width (EW similar to 185 keV) and full-width-half-maximum velocity of the broad iron line (nu >= 0.37c) necessitate an origin within d similar to 8 r(g) of the hard X-ray source. Based on the confirmed presence of a strong radio jet in this galaxy nucleus, the broad iron line may be produced in dense plasma near the base of the jet, implying that emission mechanisms in the centralmost portions of active galactic nuclei are more complex than previously thought. C1 [Brenneman, L. W.; Kadler, M.] NASA, Goddard Space Flight Ctr, CRESST, Greenbelt, MD 20771 USA. [Kadler, M.] Univ Erlangen Nurnberg, Astron Inst, D-96049 Bamberg, Germany. [Kadler, M.] Univ Space Res Assoc, Columbia, MD 21044 USA. [Marscher, A.] Boston Univ, Inst Astrophys Res, Boston, MA 02215 USA. [Ros, E.; Zensus, A.; Kovalev, Y. Y.] Max Planck Inst Radioastron, D-53010 Bonn, Germany. [Kovalev, Y. Y.] PN Lebedev Phys Inst, Ctr Astro Space, Moscow 117997, Russia. [Aller, M.; Aller, H.; Irwin, J.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Kerp, J.] Univ Bonn, Argelander Inst Astron, D-53121 Bonn, Germany. [Kaufmann, S.] Heidelberg Univ, D-69117 Heidelberg, Germany. RP Brenneman, LW (reprint author), NASA, Goddard Space Flight Ctr, CRESST, Mail Code 662, Greenbelt, MD 20771 USA. RI Tueller, Jack/D-5334-2012; Kovalev, Yuri/J-5671-2013; XRAY, SUZAKU/A-1808-2009; OI Kovalev, Yuri/0000-0001-9303-3263; Ros, Eduardo/0000-0001-9503-4892; Kadler, Matthias/0000-0001-5606-6154 FU NASA [NNX08AC226, NNX08AC22G]; Alexander von Humboldt Foundation FX B. and M. K. thank the NASA Postdoctoral Program, administered by ORAU, for their support at NASA's GSFC. K. W. gratefully acknowledges support from NASA grant NNX08AC226, M. A. from NASA grant NNX08AC22G. Y.Y.K. is a Research Fellow of the Alexander von Humboldt Foundation. L. B. and K. W. also appreciate excellent advice from Tahir Yaqoob, Chris Reynolds, Julian Krolik, Demos Kazanas, and Tim Kallman. K. W. would like to dedicate this work to Professor Andrew Wilson, who prompted her interest in LINERs and NGC 1052 in the 1990s. We gratefully acknowledge the helpful comments received from our anonymous referee, which have improved this work. NR 46 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 JUN 10 PY 2009 VL 698 IS 1 BP 528 EP 540 DI 10.1088/0004-637X/698/1/528 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 450AP UT WOS:000266373700043 ER PT J AU Liu, W Wang, TJ Dennis, BR Holman, GD AF Liu, Wei Wang, Tong-Jiang Dennis, Brian R. Holman, Gordon D. TI EPISODIC X-RAY EMISSION ACCOMPANYING THE ACTIVATION OF AN ERUPTIVE PROMINENCE: EVIDENCE OF EPISODIC MAGNETIC RECONNECTION SO ASTROPHYSICAL JOURNAL LA English DT Article DE Sun: flares; Sun: prominences; Sun: UV radiation; Sun: X-rays, gamma rays ID CORONAL MASS EJECTIONS; SOLAR-FLARES; FLUX ROPES; FILAMENT; HARD; ACCELERATION; RHESSI; ELECTRONS; ENERGY; LOOP AB We present an X-ray imaging and spectroscopic study of a partially occulted (N16W93) C7.7 flare on 2003 April 24 observed by Reuven Ramaty High Energy Solar Spectroscopy Imager that accompanied a prominence eruption observed by Transition Region and Coronal Explorer. (1) The activation and rise of the prominence occurs during the preheating phase of the flare. The initial X-ray emission appears as a single coronal source at one leg of the prominence and it then splits into a double source. Such a source splitting happens three times, each coinciding with an increased X-ray flux and plasma temperature, suggestive of fast reconnection in a localized current sheet and an enhanced energy-release rate. In the late stage of this phase, the prominence displays a helical structure. These observations are consistent with the tether-cutting and/or kink-instability model for triggering solar eruptions. (2) The eruption of the prominence takes place during the flare impulsive phase. Since then, there appear signatures predicted by the classical model of two-ribbon flares occurring in a vertical current sheet trailing an eruption. These signatures include an extreme-ultraviolet (EUV) cusp and current-sheet-like feature (or ridge) above it. There is also X-ray emission along the EUV ridge both below and above the cusp, which in both regions appears closer to the cusp at higher energies in the thermal regime (less than or similar to 20 keV). This trend is reversed in the nonthermal regime. (3) Spectral analysis indicates thermal X-rays from all sources throughout the flare, while during the impulsive phase there is additional nonthermal emission which primarily comes from the coronal source below the cusp. This source also has a lower temperature (T = 20 +/- 1 vs. 25 +/- 1 MK), a higher emission measure (EM = (3.3 +/- 0.4) vs. (1.2 +/- 0.4) x 10(47) cm(-3)), and a harder nonthermal spectrum (electron power-law index delta = 5.4 +/- 0.4 vs. 8 +/- 1) than the upper sources. C1 [Liu, Wei; Wang, Tong-Jiang; Dennis, Brian R.; Holman, Gordon D.] NASA, Goddard Space Flight Ctr, Heliophys Sci Div, Solar Phys Lab, Greenbelt, MD 20771 USA. [Wang, Tong-Jiang] Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA. RP Liu, W (reprint author), Lockheed Martin Solar & Astrophys Lab, Dept ADBS, Bldg 252,3251 Hanover St, Palo Alto, CA 94304 USA. EM weiliu@sun.stanford.edu RI Dennis, Brian/C-9511-2012; Holman, Gordon/C-9548-2012 NR 47 TC 19 Z9 19 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 JUN 10 PY 2009 VL 698 IS 1 BP 632 EP 640 DI 10.1088/0004-637X/698/1/632 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 450AP UT WOS:000266373700053 ER PT J AU Reale, F Testa, P Klimchuk, JA Parenti, S AF Reale, Fabio Testa, Paola Klimchuk, James A. Parenti, Susanna TI EVIDENCE OF WIDESPREAD HOT PLASMA IN A NONFLARING CORONAL ACTIVE REGION FROM HINODE/X-RAY TELESCOPE SO ASTROPHYSICAL JOURNAL LA English DT Article DE Sun: activity; Sun: corona; Sun: X-rays, gamma rays ID X-RAY; SOLAR CORONA; LOOPS; EMISSION; DIAGNOSTICS; MISSION AB Nanoflares, short and intense heat pulses within spatially unresolved magnetic strands, are now considered a leading candidate to solve the coronal heating problem. However, the frequent occurrence of nanoflares requires that flare-hot plasma be present in the corona at all times. Its detection has proved elusive until now, in part because the intensities are predicted to be very faint. Here, we report on the analysis of an active region observed with five filters by Hinode/X-Ray Telescope (XRT) in 2006 November. We have used the filter ratio method to derive maps of temperature and emission measure (EM) both in soft and hard ratios. These maps are approximate in that the plasma is assumed to be isothermal along each line of sight. Nonetheless, the hardest available ratio reveals the clear presence of plasma around 10 MK. To obtain more detailed information about the plasma properties, we have performed Monte Carlo simulations assuming a variety of nonisothermal EM distributions along the lines of sight. We find that the observed filter ratios imply bi-modal distributions consisting of a strong cool (log T similar to 6.3-6.5) component and a weaker (few percent) and hotter (6.6 < logT < 7.2) component. The data are consistent with bi-modal distributions along all lines of sight, i.e., throughout the active region. We also find that the isothermal temperature inferred from a filter ratio depends sensitively on the precise temperature of the cool component. A slight shift of this component can cause the hot component to be obscured in a hard ratio measurement. Consequently, temperature maps made in hard and soft ratios tend to be anti-correlated. We conclude that this observation supports the presence of widespread nanoflaring activity in the active region. C1 [Reale, Fabio] Univ Palermo, Dipartimento Sci Fis & Astron, Sez Astron, I-90134 Palermo, Italy. [Testa, Paola] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Klimchuk, James A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Parenti, Susanna] Observ Royal Belgique, B-1180 Brussels, Belgium. RP Reale, F (reprint author), INAF Osservatorio Astron Palermo GS Vaiana, Piazza Parlamento 1, I-90134 Palermo, Italy. RI Klimchuk, James/D-1041-2012; OI Klimchuk, James/0000-0003-2255-0305; Reale, Fabio/0000-0002-1820-4824 NR 23 TC 58 Z9 58 U1 2 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JUN 10 PY 2009 VL 698 IS 1 BP 756 EP 765 DI 10.1088/0004-637X/698/1/756 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 450AP UT WOS:000266373700063 ER PT J AU Frost, MI Surace, J Moustakas, LA Krick, J AF Frost, Mark I. Surace, Jason Moustakas, Leonidas A. Krick, Jessica TI A PILOT SEARCH FOR POPULATION III SUPERNOVA CANDIDATES IN THE SPITZER/IRAC DARK FIELD SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE infrared: stars; supernovae: general ID 1ST STARS; PRIMORDIAL GAS; UNIVERSE; REIONIZATION; FRAGMENTATION; FEEDBACK; NUMBER; IRAC AB We have undertaken a systematic search for candidate supernovae from high-redshift Population III stars in a field that has been observed with repeated imaging on a cadence of 2-3 weeks over a 2.2 year baseline, the Spitzer/IRAC Dark Field. The individual epochs reach a typical 5 sigma depth of 1 mu Jy in IRAC Channel 1 (3.6 mu m). Requiring a minimum of four epochs coverage, the total effective area searched is 214 arcmin(2). The unprecedented depth and multi-epochal nature of these data make it ideal for a first foray to detect transient objects which may be candidate luminous pair-instability supernovae from the primordial metallicity first stars. The search was conducted over a broad range of timescales, allowing for different durations of the putative candidates' light-curve plateau phases. All candidates were vetted by inspection of the Spitzer imaging data, as well as deep Hubble Space Telescope/Advanced Camera for Surveys F814W imaging available over the full field. While many resolved-source objects were identified with Spitzer variability, no transient objects were identified that could plausibly be identified as high-redshift supernovae candidates. The resulting 95% confidence level upper limit is 23 deg(-2) yr(-1), for sources with plateau timescales under 400/(1+z) days and brightnesses above similar to 1 mu Jy. C1 [Frost, Mark I.; Surace, Jason; Krick, Jessica] CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA. [Frost, Mark I.] Univ Sussex, Ctr Astron, Brighton BN1 9QH, E Sussex, England. [Moustakas, Leonidas A.] CALTECH, JPL, Pasadena, CA 91109 USA. RP Frost, MI (reprint author), CALTECH, Spitzer Sci Ctr, MS 220-6, Pasadena, CA 91125 USA. OI Moustakas, Leonidas/0000-0003-3030-2360 FU NASA [10521, NAS 5-26555]; STFC studentship [PPA/S/S2005/04270] FX Support for this work was provided by NASA through the Spitzer Space Telescope Visiting Graduate Student Program, through a contract issued by the Jet Propulsion Laboratory, California Institute of Technology under a contract with NASA. The work of L. A. M. was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with NASA. This research has made use of data from the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology under a contract with NASA, and the NASA/ESA Hubble Space Telescope, obtained at the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5-26555. These observations are associated with program No. 10521. Support for program No. 10521 was provided by NASA through a grant from the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5-26555. Support for this work was also provided by STFC studentship PPA/S/S2005/04270. L. A. M. is grateful to TomAbel and Ranga-Ram Chary for many discussions on this topic. We also thank Seb Oliver for his useful comments and suggestions. We are grateful to the anonymous referee for comments that have helped focus and improve this report. NR 29 TC 7 Z9 7 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD JUN 10 PY 2009 VL 698 IS 1 BP L68 EP L71 DI 10.1088/0004-637X/698/1/L68 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 450AO UT WOS:000266373600016 ER PT J AU Jackman, CH Marsh, DR Vitt, FM Garcia, RR Randall, CE Fleming, EL Frith, SM AF Jackman, Charles H. Marsh, Daniel R. Vitt, Francis M. Garcia, Rolando R. Randall, Cora E. Fleming, Eric L. Frith, Stacey M. TI Long-term middle atmospheric influence of very large solar proton events SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID 3-DIMENSIONAL MODEL SIMULATIONS; MESOSPHERIC OZONE DEPLETION; GROUND-BASED MEASUREMENTS; OCTOBER 1989; JULY 13; 2-DIMENSIONAL MODEL; STRATOSPHERIC OZONE; PARTICLE EVENTS; ODD NITROGEN; NITRIC-OXIDE AB The Whole Atmosphere Community Climate Model (WACCM3) has been used to study the long-term (more than a few months) effects of solar proton events (SPEs). Extremely large solar proton events occurred in 1972, 1989, 2000, 2001, and 2003 and caused some longer-lasting atmospheric changes. The highly energetic solar protons produced odd hydrogen (HOx) and odd nitrogen (NOy), which then led to ozone variations. Some statistically significant long-term effects on mesospheric ozone were caused by the HOx increases due to a very active time period for SPEs (years 2000-2004), even though the HOx increases were short-lived (days). The long-term stratospheric ozone effects were caused by the NOy enhancements. Very large NOy enhancements lasted for months in the middle and lower stratosphere after a few of the largest SPEs. SPE-caused NOy increases computed with WACCM3 were statistically significant at the 95% level throughout much of the polar stratosphere and mesosphere in the recent solar maximum 5-year period (2000-2004). WACCM3-computed SPE-caused polar stratospheric ozone decreases of > 10% continued for up to 5 months past the largest events; however, statistically significant ozone decreases were computed for only a relatively small fraction of this time in relatively limited altitudes in the lower mesosphere and upper stratosphere. Annually averaged model output showed statistically significant ( to 95%) stratospheric ozone loss in the polar Northern Hemisphere for years 2000-2002. The computed annually averaged temperature and total ozone change in these years were not statistically significant. C1 [Jackman, Charles H.; Fleming, Eric L.; Frith, Stacey M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Marsh, Daniel R.; Vitt, Francis M.; Garcia, Rolando R.] Natl Ctr Atmospher Res, Div Atmospher Chem, Boulder, CO 80307 USA. [Randall, Cora E.] Univ Colorado, Atmospher & Space Phys Lab, Boulder, CO 80309 USA. [Fleming, Eric L.; Frith, Stacey M.] Sci Syst & Applicat Inc, Lanham, MD USA. RP Jackman, CH (reprint author), NASA, Goddard Space Flight Ctr, Code 613-3, Greenbelt, MD 20771 USA. EM charles.h.jackman@nasa.gov; marsh@ucar.edu; fvitt@ucar.edu; rgarcia@ucar.edu; randall@lasp.colorado.edu; eric.l.fleming@nasa.gov; stacey.m.frith@nasa.gov RI Marsh, Daniel/A-8406-2008; Jackman, Charles/D-4699-2012; Randall, Cora/L-8760-2014 OI Marsh, Daniel/0000-0001-6699-494X; Randall, Cora/0000-0002-4313-4397 FU National Science Foundation FX We thank NASA Headquarters Living With a Star Targeted Research and Technology Program for support during the time that this manuscript was written. We thank the NOAA GOES team for providing the solar proton flux data over the Internet. The National Center for Atmospheric Research is sponsored by the National Science Foundation. WACCM3 results presented in this paper were generated using NASA's Columbia supercomputer housed at the NASA Ames Research Center. We thank three anonymous reviewers for valuable comments and suggestions that led to an improved manuscript. NR 58 TC 48 Z9 48 U1 1 U2 11 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 JUN 10 PY 2009 VL 114 AR D11304 DI 10.1029/2008JD011415 PG 14 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 458FU UT WOS:000267001500002 ER PT J AU Smith, MD Wolff, MJ Clancy, RT Murchie, SL AF Smith, Michael D. Wolff, Michael J. Clancy, R. Todd Murchie, Scott L. TI Compact Reconnaissance Imaging Spectrometer observations of water vapor and carbon monoxide SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Article ID THERMAL EMISSION SPECTROMETER; ART. NO. 5115; MARS ATMOSPHERE; MARTIAN ATMOSPHERE; MULTIPLE-SCATTERING; OMEGA/MARS EXPRESS; OPTICAL DEPTHS; CO; DUST; CLOUD AB The Compact Reconnaissance Imaging Spectrometer for Mars (CRISM) onboard the Mars Reconnaissance Orbiter (MRO) spacecraft began taking observations in September 2006 and has now collected more than a full Martian year of data. Retrievals performed using the near-infrared spectra obtained by CRISM are used to characterize the seasonal and spatial variation of the column abundance of water vapor and the column-averaged mixing ratio of carbon monoxide. CRISM retrievals show nominal behavior in water vapor during northern hemisphere spring and summer with maximum abundance reaching 50 precipitable micrometers. Water vapor abundance during the southern hemisphere spring and summer appears significantly reduced compared to observations by other instruments taken during previous years. The CRISM retrievals show the seasonally and globally averaged carbon monoxide mixing ratio to be 700 ppm, but with strong seasonal variations at high latitudes. The summertime near-polar carbon monoxide mixing ratio falls to 200 ppm in the south and 400 ppm in the north as carbon dioxide sublimates from the seasonal polar ice caps and dilutes noncondensable species including carbon monoxide. At low latitudes, the carbon monoxide mixing ratio varies in response to the mean seasonal cycle of surface pressure. C1 [Smith, Michael D.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Wolff, Michael J.; Clancy, R. Todd] Space Sci Inst, Boulder, CO 80301 USA. [Murchie, Scott L.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA. RP Smith, MD (reprint author), NASA, Goddard Space Flight Ctr, Mail Code 693, Greenbelt, MD 20771 USA. EM Michael.D.Smith@nasa.gov RI Smith, Michael/C-8875-2012; Murchie, Scott/E-8030-2015 OI Murchie, Scott/0000-0002-1616-8751 FU NASA FX We thank Francois Forget and Frank Lefevre for helpful comments and for making modeling results on the seasonal and spatial variation of noncondensable gases available to us before their publication. The authors acknowledge financial support from the NASA Mars Reconnaissance Orbiter project as members of the CRISM Science Team and are grateful for all the hard work done by the CRISM operations team at the Applied Physics Laboratory who performed all the sequencing and calibration needed to obtain this data set. NR 41 TC 58 Z9 58 U1 0 U2 12 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 JUN 10 PY 2009 VL 114 AR E00D03 DI 10.1029/2008JE003288 PG 13 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 458GH UT WOS:000267003000001 ER PT J AU Han, SC Mazarico, E Lemoine, FG AF Han, Shin-Chan Mazarico, Erwan Lemoine, Frank G. TI Improved nearside gravity field of the Moon by localizing the power law constraint SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID KAGUYA; MODEL AB The problem associated with the large data gap on the farside of the Moon is addressed for constructing a high-resolution global gravity model. By localizing the power law constraint and making it effective only within the farside and limb regions, we mitigate the undesired power-limiting effect on the nearside. Compared to the solution estimated from Lunar Prospector and other satellite tracking data with the globally-applied power law, the locally-constrained solution shows significant improvement of the nearside gravity estimates. Around the areas dominated by craters in the southern hemisphere of the nearside, the correlation with topography approaches nearly 0.95 and the admittance converges to 100110 mGal/km up to spherical harmonic degree 130, while the globally-constrained solutions distort starting at degree 90. The proposed analysis can benefit the science and operation of other existing and future planetary missions and enhance the geophysical interpretation of the gravity field. Citation: Han, S.-C., E. Mazarico, and F. G. Lemoine (2009), Improved nearside gravity field of the Moon by localizing the power law constraint, Geophys. Res. Lett., 36, L11203, doi: 10.1029/2009GL038556. C1 [Han, Shin-Chan; Mazarico, Erwan; Lemoine, Frank G.] NASA, Goddard Space Flight Ctr, Planetary Geodynam Lab, Greenbelt, MD 20771 USA. [Han, Shin-Chan] Univ Maryland Baltimore Cty, GEST, Baltimore, MD 21228 USA. [Mazarico, Erwan] ORAU NASA Postdoctoral Program, Washington, DC USA. RP Han, SC (reprint author), NASA, Goddard Space Flight Ctr, Planetary Geodynam Lab, Code 698, Greenbelt, MD 20771 USA. EM shin-chan.han@nasa.gov RI Lemoine, Frank/D-1215-2013; Han, Shin-Chan/A-2022-2009; Mazarico, Erwan/N-6034-2014 OI Mazarico, Erwan/0000-0003-3456-427X NR 15 TC 11 Z9 12 U1 0 U2 1 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 JUN 9 PY 2009 VL 36 AR L11203 DI 10.1029/2009GL038556 PG 5 WC Geosciences, Multidisciplinary SC Geology GA 458FH UT WOS:000267000000007 ER PT J AU Xu, TB Guerreiro, N Hubbard, J Kang, JH Park, C Harrison, J AF Xu, Tian-Bing Guerreiro, Nelson Hubbard, James Kang, Jin Ho Park, Cheol Harrison, Joycelyn TI One-dimensional contact mode interdigitated center of pressure sensor SO APPLIED PHYSICS LETTERS LA English DT Article DE pressure sensors AB A one-dimensional contact mode interdigitated center of pressure sensor (CMIPS) has been developed. The experimental study demonstrated that the CMIPS has the capability to measure the overall pressure as well as the center of pressure in one dimension simultaneously. A theoretical model for the CMIPS is established here based on the equivalent circuit of the configuration of the CMIPS as well as the material properties of the sensor. The experimental results match well with theoretical modeling predictions. A system mapped with two or more pieces of the CMIPS can be used to obtain information from the pressure distribution in multidimensions. C1 [Xu, Tian-Bing; Guerreiro, Nelson; Hubbard, James; Kang, Jin Ho; Park, Cheol] Natl Inst Aerosp, Hampton, VA 23666 USA. [Guerreiro, Nelson; Hubbard, James] Univ Maryland, College Pk, MD 20742 USA. [Harrison, Joycelyn] NASA, Langley Res Ctr, Hampton, VA 23681 USA. [Park, Cheol] Univ Virginia, Dept Mech & Aerosp Engn, Charlottesville, VA 22904 USA. RP Xu, TB (reprint author), Natl Inst Aerosp, 100 Explorat Way, Hampton, VA 23666 USA. EM tbxu@nianet.org NR 8 TC 3 Z9 3 U1 0 U2 2 PU AMER INST PHYSICS PI MELVILLE PA CIRCULATION & FULFILLMENT DIV, 2 HUNTINGTON QUADRANGLE, STE 1 N O 1, MELVILLE, NY 11747-4501 USA SN 0003-6951 J9 APPL PHYS LETT JI Appl. Phys. Lett. PD JUN 8 PY 2009 VL 94 IS 23 AR 233503 DI 10.1063/1.3152010 PG 3 WC Physics, Applied SC Physics GA 457ZH UT WOS:000266977100092 ER PT J AU Cadonati, L Aylott, B Baker, JG Boggs, WD Boyle, M Brady, PR Brown, DA Brugmann, B Buchman, LT Buonanno, A Camp, J Campanelli, M Centrella, J Chatterji, S Christensen, N Chu, T Diener, P Dorband, N Etienne, ZB Faber, J Fairhurst, S Farr, B Fischetti, S Guidi, G Goggin, LM Hannam, M Herrmann, F Hinder, I Husa, S Kalogera, V Keppel, D Kidder, LE Kelly, BJ Krishnan, B Laguna, P Lousto, CO Mandel, I Marronetti, P Matzner, R McWilliams, ST Matthews, KD Mercer, RA Mohapatra, SRP Mroue, AH Nakano, H Ochsner, E Pan, Y Pekowsky, L Pfeiffer, HP Pollney, D Pretorius, F Raymond, V Reisswig, C Rezzolla, L Rinne, O Robinson, C Rover, C Santamaria, L Sathyaprakash, B Scheel, MA Schnetter, E Seiler, J Shapiro, SL Shoemaker, D Sperhake, U Stroeer, A Sturani, R Tichy, W Liu, YT van der Sluys, M van Meter, JR Vaulin, R Vecchio, A Veitch, J Vicere, A Whelan, JT Zlochower, Y AF Cadonati, Laura Aylott, Benjamin Baker, John G. Boggs, William D. Boyle, Michael Brady, Patrick R. Brown, Duncan A. Bruegmann, Bernd Buchman, Luisa T. Buonanno, Alessandra Camp, Jordan Campanelli, Manuela Centrella, Joan Chatterji, Shourov Christensen, Nelson Chu, Tony Diener, Peter Dorband, Nils Etienne, Zachariah B. Faber, Joshua Fairhurst, Stephen Farr, Benjamin Fischetti, Sebastian Guidi, Gianluca Goggin, Lisa M. Hannam, Mark Herrmann, Frank Hinder, Ian Husa, Sascha Kalogera, Vicky Keppel, Drew Kidder, Lawrence E. Kelly, Bernard J. Krishnan, Badri Laguna, Pablo Lousto, Carlos O. Mandel, Ilya Marronetti, Pedro Matzner, Richard McWilliams, Sean T. Matthews, Keith D. Mercer, R. Adam Mohapatra, Satyanarayan R. P. Mroue, Abdul H. Nakano, Hiroyuki Ochsner, Evan Pan, Yi Pekowsky, Larne Pfeiffer, Harald P. Pollney, Denis Pretorius, Frans Raymond, Vivien Reisswig, Christian Rezzolla, Luciano Rinne, Oliver Robinson, Craig Roever, Christian Santamaria, Lucia Sathyaprakash, Bangalore Scheel, Mark A. Schnetter, Erik Seiler, Jennifer Shapiro, Stuart L. Shoemaker, Deirdre Sperhake, Ulrich Stroeer, Alexander Sturani, Riccardo Tichy, Wolfgang Liu, Yuk Tung van der Sluys, Marc van Meter, James R. Vaulin, Ruslan Vecchio, Alberto Veitch, John Vicere, Andrea Whelan, John T. Zlochower, Yosef TI Status of NINJA: the Numerical INJection Analysis project SO CLASSICAL AND QUANTUM GRAVITY LA English DT Article; Proceedings Paper CT Numerical Relativity Data Analysis Meeting CY MAY 11-AUG 14, 2008 CL Syracuse Univ, Dept Phys, Syracuse, NY HO Syracuse Univ, Dept Phys ID BLACK-HOLE BINARIES; GRAVITATIONAL-WAVE BURSTS; MODELING KICKS; SCIENCE RUN; SEARCH; RELATIVITY; MERGER; SPIN; DECOMPOSITION; PERTURBATIONS AB The 2008 NRDA conference introduced the Numerical INJection Analysis project (NINJA), a new collaborative effort between the numerical relativity community and the data analysis community. NINJA focuses on modeling and searching for gravitational wave signatures from the coalescence of binary system of compact objects. We review the scope of this collaboration and the components of the first NINJA project, where numerical relativity groups, shared waveforms and data analysis teams applied various techniques to detect them when embedded in colored Gaussian noise. C1 [Aylott, Benjamin; Vecchio, Alberto; Veitch, John] Univ Birmingham, Sch Phys & Astron, Birmingham B15 2TT, W Midlands, England. [Baker, John G.; Camp, Jordan; Centrella, Joan; Kelly, Bernard J.; McWilliams, Sean T.; van Meter, James R.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Boggs, William D.; Ochsner, Evan; Pan, Yi] Univ Maryland, Maryland Ctr Fundamental Phys, Dept Phys, College Pk, MD 20742 USA. [Brady, Patrick R.; Goggin, Lisa M.; Mercer, R. Adam; Vaulin, Ruslan] Univ Wisconsin, Milwaukee, WI 53201 USA. [Brown, Duncan A.; Pekowsky, Larne] Syracuse Univ, Dept Phys, Syracuse, NY 13254 USA. [Bruegmann, Bernd; Sperhake, Ulrich] Univ Jena, Inst Theoret Phys, D-07743 Jena, Germany. [Cadonati, Laura; Fischetti, Sebastian; Mohapatra, Satyanarayan R. P.] Univ Massachusetts, Dept Phys, Amherst, MA 01003 USA. [Campanelli, Manuela; Faber, Joshua; Farr, Benjamin; Lousto, Carlos O.; Nakano, Hiroyuki; Whelan, John T.; Zlochower, Yosef] Rochester Inst Technol, Ctr Computat Relat & Gravitat, Rochester, NY 14623 USA. [Campanelli, Manuela; Faber, Joshua; Farr, Benjamin; Lousto, Carlos O.; Nakano, Hiroyuki; Whelan, John T.; Zlochower, Yosef] Rochester Inst Technol, Sch Math Sci, Rochester, NY 14623 USA. [Chatterji, Shourov; Guidi, Gianluca; Sturani, Riccardo; Vicere, Andrea] INFN Sez Firenze Urbino, I-50019 Sesto Fiorentino, Italy. [Chatterji, Shourov; Keppel, Drew] CALTECH, LIGO, Pasadena, CA 91125 USA. [Christensen, Nelson; Robinson, Craig] Carleton Coll, Northfield, MN 55057 USA. [Diener, Peter; Schnetter, Erik] Louisiana State Univ, Ctr Computat & Technol, Baton Rouge, LA 70803 USA. [Diener, Peter; Schnetter, Erik] Louisiana State Univ, Dept Phys & Astron, Baton Rouge, LA 70803 USA. [Dorband, Nils; Husa, Sascha; Krishnan, Badri; Pollney, Denis; Reisswig, Christian; Rezzolla, Luciano; Santamaria, Lucia; Seiler, Jennifer; Whelan, John T.] Max Planck Inst Gravitat Phys, D-14476 Potsdam, Germany. [Etienne, Zachariah B.; Shapiro, Stuart L.; Liu, Yuk Tung] Univ Illinois, Dept Phys, Urbana, IL 61801 USA. [Fairhurst, Stephen; Farr, Benjamin; Sathyaprakash, Bangalore] Cardiff Univ, Sch Phys & Astron, Cardiff, S Glam, Wales. [Guidi, Gianluca; Sturani, Riccardo; Vicere, Andrea] Univ Urbino, Ist Fis, I-61029 Urbino, Italy. [Hannam, Mark] Natl Univ Ireland Univ Coll Cork, Dept Phys, Cork, Ireland. [Herrmann, Frank; Hinder, Ian] Penn State Univ, Ctr Gravitat Wave Phys, University Pk, PA 16802 USA. [Herrmann, Frank] Univ Maryland, Ctr Sci Computat & Math Modeling, College Pk, MD 20742 USA. [Husa, Sascha] Univ Illes Balears, Dept Fis, E-07071 Palma de Mallorca, Spain. [Mandel, Ilya; Raymond, Vivien; van der Sluys, Marc] Northwestern Univ, Dept Phys & Astron, Evanston, IL USA. [Kidder, Lawrence E.; Mroue, Abdul H.] Cornell Univ, Ctr Radiophys & Space Res, Ithaca, NY 14853 USA. [Laguna, Pablo; Shoemaker, Deirdre] Georgia Inst Technol, Ctr Relativist Astrophys & Sch Phys, Atlanta, GA 30332 USA. [Marronetti, Pedro; Tichy, Wolfgang] Florida Atlantic Univ, Dept Phys, Boca Raton, FL 33431 USA. [Matzner, Richard] Univ Texas Austin, Austin, TX 78712 USA. [Pretorius, Frans] Princeton Univ, Dept Phys, Princeton, NJ 08540 USA. [Rinne, Oliver] Ctr Math Sci, Dept Appl Math & Theoret Phys, Cambridge CB3 0WA, England. [Rinne, Oliver] Kings Coll London, Cambridge CB2 1ST, England. [Roever, Christian] Max Planck Inst Gavitat Phys, Hannover, Germany. [Stroeer, Alexander] Univ Maryland, CRESST, College Pk, MD 20742 USA. RP Cadonati, L (reprint author), Univ Birmingham, Sch Phys & Astron, Birmingham B15 2TT, W Midlands, England. RI van meter, james/E-7893-2011; Kelly, Bernard/G-7371-2011; Santamaria, Lucia/A-7269-2012; Vicere, Andrea/J-1742-2012; Vecchio, Alberto/F-8310-2015; Hinder, Ian/J-5002-2014; OI Guidi, Gianluca/0000-0002-3061-9870; Santamaria, Lucia/0000-0002-5986-0449; Lousto, Carlos/0000-0002-6400-9640; Schnetter, Erik/0000-0002-4518-9017; Kelly, Bernard/0000-0002-3326-4454; Reisswig, Christian/0000-0001-6855-9351; Mandel, Ilya/0000-0002-6134-8946; Veitch, John/0000-0002-6508-0713; Nakano, Hiroyuki/0000-0001-7665-0796; Husa, Sascha/0000-0002-0445-1971; Farr, Ben/0000-0002-2916-9200; Vicere, Andrea/0000-0003-0624-6231; Vecchio, Alberto/0000-0002-6254-1617; Rover, Christian/0000-0002-6911-698X; Seiler, Jennifer/0000-0003-2855-3945; Hinder, Ian/0000-0003-3548-9101; Whelan, John/0000-0001-5710-6576; Fairhurst, Stephen/0000-0001-8480-1961 NR 120 TC 11 Z9 11 U1 0 U2 16 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0264-9381 EI 1361-6382 J9 CLASSICAL QUANT GRAV JI Class. Quantum Gravity PD JUN 7 PY 2009 VL 26 IS 11 AR 114008 DI 10.1088/0264-9381/26/11/114008 PG 13 WC Astronomy & Astrophysics; Physics, Multidisciplinary; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA 447RA UT WOS:000266208300009 ER PT J AU Stroeer, A Camp, J AF Stroeer, Alexander Camp, Jordan TI NINJA data analysis with a detection pipeline based on the Hilbert-Huang transform SO CLASSICAL AND QUANTUM GRAVITY LA English DT Article; Proceedings Paper CT Numerical Relativity Data Analysis Meeting CY MAY 11-AUG 14, 2008 CL Syracuse Univ, Dept Phys, Syracuse, NY HO Syracuse Univ, Dept Phys ID GRAVITATIONAL-WAVE DETECTION; NUMERICAL RELATIVITY AB The NINJA data analysis challenge allowed the study of the sensitivity of data analysis pipelines to binary black hole numerical relativity waveforms in simulated Gaussian noise at the design level of the LIGO observatory and the VIRGO observatory. We analyzed NINJA data with a pipeline based on the Hilbert-Huang transform, utilizing a detection stage and a characterization stage: detection is performed by triggering on excess instantaneous power, characterization is performed by displaying the kernel density enhanced (KD) time-frequency trace of the signal. Using the simulated data based on the two LIGO detectors, we were able to detect 77 signals out of 126 above signal-to-noise ratio, SNR 5 in coincidence, with 43 missed events characterized by SNR < 10. Characterization of the detected signals revealed the merger part of the waveform in high time and frequency resolution, free from time frequency uncertainty. We estimated the timelag of the signals between the detectors based on the optimal overlap of the individual KD time-frequency maps, yielding estimates accurate within a fraction of a millisecond for half of the events. A coherent addition of the data sets according to the estimated timelag eventually was used in a final characterization of the event. C1 [Stroeer, Alexander; Camp, Jordan] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Stroeer, Alexander] Univ Maryland, CRESST, College Pk, MD 20742 USA. RP Stroeer, A (reprint author), NASA, Goddard Space Flight Ctr, Code 663, Greenbelt, MD 20771 USA. EM Alexander.Stroeer@nasa.gov NR 34 TC 3 Z9 3 U1 0 U2 4 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 JUN 7 PY 2009 VL 26 IS 11 AR 114012 DI 10.1088/0264-9381/26/11/114012 PG 9 WC Astronomy & Astrophysics; Physics, Multidisciplinary; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA 447RA UT WOS:000266208300013 ER PT J AU Milliken, RE Fischer, WW Hurowitz, JA AF Milliken, R. E. Fischer, W. W. Hurowitz, J. A. TI Missing salts on early Mars SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID SILICATE MINERALS; MAWRTH-VALLIS; CLAY-MINERALS; DISSOLUTION; CRATER; PH; PHYLLOSILICATES; IDENTIFICATION; TEMPERATURE; MECHANISM AB Our understanding of the role of water on Mars has been profoundly influenced over the past several years by the detection of widespread aqueous alteration minerals. Clay minerals are found throughout ancient Noachian terrains and sulfate salts are abundant in younger Hesperian terrains, but these phases are rarely found together in the early Martian rock record. Full alteration assemblages are generally not recognized at local scales, hindering our ability to close mass balance in the ancient crust. Here we demonstrate the dissolution of basalt and subsequent formation of smectite results in an excess of cations that should reside with anions such as OH(-), Cl(-), SO(3)(2-), SO(4)(2-), or CO(3)(2-) in a significant reservoir of complementary salts. Such salts are largely absent from Noachian terrains, yet the composition and/or fate of these 'missing salts' is critical to understanding the oxidation state and primary atmospheric volatile involved in crustal weathering on early Mars. Citation: Milliken, R. E., W. W. Fischer, and J. A. Hurowitz (2009), Missing salts on early Mars, Geophys. Res. Lett., 36, L11202, doi: 10.1029/2009GL038558. C1 [Milliken, R. E.; Hurowitz, J. A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Fischer, W. W.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. RP Milliken, RE (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM ralph.milliken@jpl.nasa.gov FU NASA FX The research described in this paper was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with NASA. We thank Nick Tosca and anonymous reviewer for comments that improved this manuscript. NR 32 TC 30 Z9 30 U1 2 U2 5 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD JUN 6 PY 2009 VL 36 AR L11202 DI 10.1029/2009GL038558 PG 5 WC Geosciences, Multidisciplinary SC Geology GA 455EW UT WOS:000266741900006 ER PT J AU Alexandrov, N AF Alexandrov, Natalia TI Your virtual twin SO NEW SCIENTIST LA English DT Editorial Material C1 NASA, Langley Res Ctr, Hampton, VA 23665 USA. RP Alexandrov, N (reprint author), NASA, Langley Res Ctr, Hampton, VA 23665 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 JUN 6 PY 2009 VL 202 IS 2711 BP 28 EP 28 PG 1 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 456LM UT WOS:000266847800034 ER PT J AU Loeb, NG Wielicki, BA Wong, T Parker, PA AF Loeb, Norman G. Wielicki, Bruce A. Wong, Takmeng Parker, Peter A. TI Impact of data gaps on satellite broadband radiation records SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID BUDGET; CERES AB A simulated 30-year climate data record of net cloud radiative effect (defined as the difference between clear- and all-sky net top-of-atmosphere radiative flux) based on the first 5 years of Clouds and the Earth's Radiant Energy System (CERES) Terra measurements is created in order to investigate how gaps in the record affect our ability to constrain cloud radiative feedback. To ensure a trend estimate with an uncertainty small enough to constrain cloud radiative feedback to 25% of anthropogenic forcing in the next few decades, the absolute calibration change across the gap must be <0.3% in the shortwave (SW) region and <0.1% in the longwave (LW) region for a 1-year gap occurring in the middle of the record. Given that current calibration accuracy of CERES is 2% in the SW and 1% in the LW (at the 95% significance level), a gap of any length anywhere in the record will significantly increase the time required in order to detect a trend above natural variability because data collected prior to and after the gap cannot be combined accurately enough to ensure trend detection at the required level. To avoid gaps, at least 6 months of global or 1 year of tropical overlapping measurements between successive instruments are needed, based on overlapping CERES Terra and Aqua data. C1 [Loeb, Norman G.; Wielicki, Bruce A.; Wong, Takmeng; Parker, Peter A.] NASA, Langley Res Ctr, Hampton, VA 23681 USA. RP Loeb, NG (reprint author), NASA, Langley Res Ctr, Mail Stop 420, Hampton, VA 23681 USA. EM norman.g.loeb@nasa.gov FU NASA Science Mission Directorate FX We would like to thank Betsy Weatherhead for her careful and thoughtful review of the paper. The CERES data are provided by the NASA Langley Atmospheric Sciences Data Center in Hampton, Virginia. The NASA Science Mission Directorate through the CERES project at Langley Research Center funded this study. NR 14 TC 7 Z9 7 U1 2 U2 10 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 JUN 5 PY 2009 VL 114 AR D11109 DI 10.1029/2008JD011183 PG 7 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 455FC UT WOS:000266742500002 ER PT J AU Xie, Y Yang, P Kattawar, GW Minnis, P Hu, YX AF Xie, Yu Yang, Ping Kattawar, George W. Minnis, Patrick Hu, Yong X. TI Effect of the inhomogeneity of ice crystals on retrieving ice cloud optical thickness and effective particle size SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID SINGLE-SCATTERING PROPERTIES; SATELLITE-BASED RETRIEVAL; DIFFERENCE TIME-DOMAIN; LIGHT-SCATTERING; CIRRUS CLOUDS; RADIATIVE-TRANSFER; SURFACE-ROUGHNESS; BULLET ROSETTES; MODELS; MATRICES AB Spherical or spheroidal air bubbles are often trapped in rapidly growing ice crystals. In this study, the single-scattering properties of inhomogeneous ice crystals containing air bubbles are investigated. Specifically, a combination of the ray-tracing technique and the Monte Carlo method is used to simulate the scattering of light by randomly oriented large hexagonal ice crystals containing spherical or spheroidal air bubbles. The effect of the air bubbles within ice crystals is to smooth the phase functions, diminish the 22 degrees and 46 degrees halo peaks, and reduce the backscatter in comparison with the case of bubble-free ice crystals. These features vary with the number, sizes, locations, and shapes of the air bubbles within the ice crystals. Moreover, the asymmetry factors of inhomogeneous ice crystals decrease as the ratio of air-bubble volume to ice crystal volume increases. Cloud reflectance look-up tables were generated at the wavelengths of 0.65 mu m and 2.13 mu m to examine the impact of accounting for air bubbles in ice crystal morphology on the retrieval of ice cloud optical thickness and effective particle size. The reflectances simulated for inhomogeneous ice crystals are larger than those computed for homogeneous ice crystals at a wavelength of 0.65 mu m. Thus the retrieved cloud optical thickness is reduced by employing inhomogeneous ice cloud models. At a wavelength of 2.13 mu m, including air bubbles in ice crystal morphology may also increase the reflectance. This effect implies, particularly in the case of large air bubbles, that the retrieved effective particle size for inhomogeneous ice crystals is larger than that retrieved for homogeneous ice crystals. C1 [Xie, Yu; Yang, Ping] Texas A&M Univ, Dept Atmospher Sci, College Stn, TX 77843 USA. [Minnis, Patrick; Hu, Yong X.] NASA, Langley Res Ctr, Hampton, VA 23681 USA. [Kattawar, George W.] Texas A&M Univ, Dept Phys, College Stn, TX 77843 USA. RP Xie, Y (reprint author), Texas A&M Univ, Dept Atmospher Sci, College Stn, TX 77843 USA. EM xieyu@ariel.met.tamu.edu RI Xie, Yu/A-4266-2011; Yang, Ping/B-4590-2011; Minnis, Patrick/G-1902-2010; Hu, Yongxiang/K-4426-2012 OI Minnis, Patrick/0000-0002-4733-6148; FU National Science Foundation (NSF) [ATM-0239605]; NASA [NNL06AA23G]; Office of Naval Research [N00014-06-1-0069]; NASA Radiation Sciences; NASA Clouds and the Earth's Radiant Energy System Project FX This research is supported by a National Science Foundation (NSF) grant (ATM-0239605) managed by Bradley Smull and by a NASA grant (NNL06AA23G). George W. Kattawar's research is also supported by the Office of Naval Research under contract N00014-06-1-0069. Patrick Minnis is supported through the NASA Radiation Sciences Program and the NASA Clouds and the Earth's Radiant Energy System Project. NR 44 TC 21 Z9 21 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 JUN 5 PY 2009 VL 114 AR D11203 DI 10.1029/2008JD011216 PG 12 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 455FC UT WOS:000266742500003 ER PT J AU Mende, SB Frey, HU McFadden, J Carlson, CW Angelopoulos, V Glassmeier, KH Sibeck, DG Weatherwax, A AF Mende, S. B. Frey, H. U. McFadden, J. Carlson, C. W. Angelopoulos, V. Glassmeier, K. -H. Sibeck, D. G. Weatherwax, A. TI Coordinated observation of the dayside magnetospheric entry and exit of the THEMIS satellites with ground-based auroral imaging in Antarctica SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article ID FLUX-TRANSFER EVENTS; PLASMA CONVECTION; SOUTH-POLE; SIGNATURES; MAGNETOPAUSE; FORMS; MAGNETOSHEATH; MAGNETOMETER; MOMENTUM; DYNAMICS AB Data from the five-satellite Time History of Events and Macroscale Interactions during Substorms (THEMIS) constellation suitably located to study solar wind magnetospheric coupling during the austral winter of 2007 were compared to data from ground-based all-sky imagers (ASIs) at South Pole (74 degrees magnetic latitude) and at AGO-1 (80 degrees magnetic latitude). The THEMIS constellation entered and exited the magnetosphere near magnetic midday on 10 and 12 August 2007, respectively. On 12 August interplanetary magnetic field (IMF) (B(z) > 0) the dayside aurora was located more poleward between AGO-1 and South Pole. The THEMIS satellites traversing the magnetopause saw it move in and out several times during the satellite crossings. The inward motion of the magnetopause was sometimes correlated with equatorward expansions of the aurora and sometimes with solar wind pressure pulses as seen by Geotail. The Bz > 0 auroral latitude was consistent with dayside cusp "spot'' seen by the IMAGE spacecraft and had been associated with footprints of "steady state'' lobe reconnection. The aurora consisted of a continuous stream of poleward moving auroral forms (PMAF) even during a period of slightly B(z) > 0 and B(y) = 0. On 10 August 2007 IMF B(z) < 0 the dayside aurora was located more equatorward, over South Pole, and the THEMIS satellites crossed the bow shock from the magnetosheath into the solar wind. Negative Bz pulses observed at the satellite were correlated with large poleward expansions of the dayside aurora consistent with reconnection in the subsolar region accompanied by simultaneous plasma density increases at THEMIS B satellite consistent with outward radial motion of the bow shock. C1 [Mende, S. B.; Frey, H. U.; McFadden, J.; Carlson, C. W.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Angelopoulos, V.] Univ Calif Los Angeles, Dept Earth & Space Sci, Inst Geophys & Planetary Phys, Los Angeles, CA 90095 USA. [Glassmeier, K. -H.] Tech Univ Carolo Wilhelmina Braunschweig, Inst Geophys & Extraterr Phys, D-38106 Braunschweig, Germany. [Sibeck, D. G.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Weatherwax, A.] Siena Coll, Dept Phys, Loudonville, NY 12211 USA. RP Mende, SB (reprint author), Univ Calif Berkeley, Space Sci Lab, 7 Gauss Way, Berkeley, CA 94720 USA. EM mende@ssl.berkeley.edu RI Sibeck, David/D-4424-2012; OI Frey, Harald/0000-0001-8955-3282 FU NASA [NAS502099]; NSF [0636899, 0340845] FX The authors gratefully acknowledge the outstanding accomplishments of the THEMIS engineering and science team. The THEMIS program was supported by NASA under contract NAS502099. The data collection from Antarctica was made possible by the Antarctic program funded by NSF under grants 0636899 and 0340845. The authors are also greatly indebted to all those who worked for many years on the U. S. Antarctic Automatic Geophysical Observatory program, including William Rachelson, Stewart Harris, and J. Doolittle. Data from Geotail through the courtesy of T. Mukai and S. Kokubun are gratefully acknowledged. Similarly, we acknowledge N. Ness at the Bartol Research Institute for providing the ACE magnetic field data. NR 24 TC 5 Z9 5 U1 0 U2 2 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0148-0227 J9 J GEOPHYS RES-SPACE JI J. Geophys. Res-Space Phys. PD JUN 5 PY 2009 VL 114 AR A00C23 DI 10.1029/2008JA013496 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 455GS UT WOS:000266747100001 ER PT J AU Clancy, TC Frankland, SJV Hinkley, JA Gates, TS AF Clancy, T. C. Frankland, S. J. V. Hinkley, J. A. Gates, T. S. TI Molecular modeling for calculation of mechanical properties of epoxies with moisture ingress SO POLYMER LA English DT Article DE Epoxy; Simulation; Mechanical properties ID DYNAMICS SIMULATION; GLASS-TRANSITION; PART II; WATER; RESIN; POLYMER; DEFORMATION; PREDICTION; ABSORPTION; ADHESIVE AB Atomistic models of epoxy structures were built in order to assess the effect of crosslink degree, moisture content and temperature on the calculated properties of a typical representative generic epoxy. Each atomistic model had approximately 7000 atoms and was contained within a periodic boundary condition cell with edge lengths of about 4 nm. Four atomistic models were built with a range of crosslink degree and moisture content. Each of these structures was simulated at three temperatures: 300 K, 350 K, and 400 K. Elastic constants were calculated for these structures by monitoring the stress tensor as a function of applied strain deformations to the periodic boundary conditions. The mechanical properties showed reasonably consistent behavior with respect to these parameters. The moduli decreased with decreasing crosslink degree and with increasing temperature. The moduli generally decreased with increasing moisture content, although this effect was not as consistent as that seen for temperature and crosslink degree. (c) 2009 Elsevier Ltd. All rights reserved. C1 [Clancy, T. C.; Frankland, S. J. V.] Natl Inst Aerosp, Hampton, VA 23666 USA. [Hinkley, J. A.; Gates, T. S.] NASA, Langley Res Ctr, Hampton, VA 23681 USA. RP Clancy, TC (reprint author), Natl Inst Aerosp, 100 Explorat Way, Hampton, VA 23666 USA. EM Thomas.C.Clancy@nasa.gov FU Aging Aircraft and Durability; Aviation Safety Program of the National Aeronautics and Space Administration FX This work was funded by the Aging Aircraft and Durability Project as part of the Aviation Safety Program of the National Aeronautics and Space Administration. NR 23 TC 34 Z9 34 U1 0 U2 27 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 0032-3861 J9 POLYMER JI Polymer PD JUN 5 PY 2009 VL 50 IS 12 BP 2736 EP 2742 DI 10.1016/j.polymer.2009.04.021 PG 7 WC Polymer Science SC Polymer Science GA 454TY UT WOS:000266706800027 ER PT J AU Kim, C Hwang, SJ Bowman, RC Reiter, JW Zan, JA Kulleck, JG Kabbour, H Majzoub, EH Ozolins, V AF Kim, Chul Hwang, Son-Jong Bowman, Robert C., Jr. Reiter, Joseph W. Zan, Jason A. Kulleck, James G. Kabbour, Houria Majzoub, E. H. Ozolins, V. TI LiSc(BH4)(4) as a Hydrogen Storage Material: Multinuclear High-Resolution Solid-State NMR and First-Principles Density Functional Theory Studies SO JOURNAL OF PHYSICAL CHEMISTRY C LA English DT Article ID TOTAL-ENERGY CALCULATIONS; AUGMENTED-WAVE METHOD; N-H SYSTEM; METAL-BOROHYDRIDES; THERMODYNAMICAL STABILITIES; CROSS-POLARIZATION; CRYSTAL-STRUCTURES; BASIS-SET; LIBH4; MG AB A lithium salt of anionic scandium tetraborohydride complex, LiSc(BH4)(4), was studied both experimentally and theoretically as a potential hydrogen storage medium. Ball milling mixtures of LiBH4 and SCCL3 produced LCl and a unique crystalline hydride, which has been unequivocally identified via multinuclear solid-state nuclear magnetic resonance (NMR) to be LiSc(BH4)(4), Under the present reaction conditions, there was no evidence for the formation of binary Sc(BH4)(3). These observations are in agreement with our first-principles calculations of the relative stabilities of these phases. A tetragonal structure in space group I (4) over bar (#82) is predicted to be the lowest energy state for LiSc(BH4)(4), which does not correspond to structures obtained to date on the crystalline ternary borohydride phases made by ball milling. Perhaps reaction conditions are resulting in formation of other polymorphs, which should be investigated in future studies via neutron scattering on deuterides. Hydrogen desorption while heating these Li-Sc-B-H materials up to 400 degrees C yielded only amorphous phases (besides the virtually unchanged LiCl) that were deter-mined by NMR to be primarily ScB2 and [B12H12](-2) anion containing (e.g., Li2B12H12) along with residual LiBH4. Reaction of a desorbed LiSc(BH4)(4) + 4LiCl mixture (from 4LiBH(4)/ScCl3 sample) with hydrogen gas at similar to 70 bar resulted only in an increase in the contents of Li2B12H12 and LiBH4. Full reversibility to reform the LiSc(BH4)(4) was not found. Overall, the Li-Sc-B-H system is not a favorable candidate for hydrogen storage applications. C1 [Kim, Chul; Hwang, Son-Jong] CALTECH, Div Chem & Chem Engn, Pasadena, CA 91125 USA. [Bowman, Robert C., Jr.; Reiter, Joseph W.; Zan, Jason A.; Kulleck, James G.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Kabbour, Houria] CALTECH, Div Engn & Appl Sci, Pasadena, CA 91125 USA. [Majzoub, E. H.] Univ Missouri, Ctr Nanosci, St Louis, MO 63121 USA. [Majzoub, E. H.] Univ Missouri, Dept Phys & Astron, St Louis, MO 63121 USA. [Ozolins, V.] Univ Calif Los Angeles, Dept Mat Sci & Engn, Los Angeles, CA 90095 USA. RP Hwang, SJ (reprint author), CALTECH, Div Chem & Chem Engn, Pasadena, CA 91125 USA. EM sonjong@cheme.caltech.edu RI Ozolins, Vidvuds/D-4578-2009 FU DOE [DE-AI-01-05EE11105, DE-FC36-05GO15065]; National Science Foundation (NSF) [9724240, DMR-0520565]; U.S. Department of Energy [DE-FG0207ER46433]; DOE INCITE program; U.S. Department of Energy, Office of Energy Efficiency and Renewable Energy, in the Hydrogen, Fuel Cells & Infrastructure Technologies Program [DE-AC04-94AL8500] FX We thank Dr. Charming Alm for his contributions and support. This research was partially performed at the Jet Propulsion Laboratory, which is operated by the California Institute of Technology under contract with the NASA. This work was partially supported by DOE through Award Nos. DE-AI-01-05EE11105 and DE-FC36-05GO15065. The NMR facility at Caltech was supported by the National Science Foundation (NSF) under Grant No. 9724240 and partially supported by the MRSEC Program of the NSF under Award No. DMR-0520565. Research at UCLA was supported by the U.S. Department of Energy under grant No. DE-FG0207ER46433 and by the DOE INCITE program. Research at UMSL was funded by the U.S. Department of Energy, Office of Energy Efficiency and Renewable Energy, in the Hydrogen, Fuel Cells & Infrastructure Technologies Program under Contract No. DE-AC04-94AL8500. NR 50 TC 46 Z9 46 U1 0 U2 23 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 JUN 4 PY 2009 VL 113 IS 22 BP 9956 EP 9968 DI 10.1021/jp9011685 PG 13 WC Chemistry, Physical; Nanoscience & Nanotechnology; Materials Science, Multidisciplinary SC Chemistry; Science & Technology - Other Topics; Materials Science GA 451CF UT WOS:000266447600076 ER PT J AU Rodriguez, S Le Mouelic, S Rannou, P Tobie, G Baines, KH Barnes, JW Griffith, CA Hirtzig, M Pitman, KM Sotin, C Brown, RH Buratti, BJ Clark, RN Nicholson, PD AF Rodriguez, Sebastien Le Mouelic, Stephane Rannou, Pascal Tobie, Gabriel Baines, Kevin H. Barnes, Jason W. Griffith, Caitlin A. Hirtzig, Mathieu Pitman, Karly M. Sotin, Christophe Brown, Robert H. Buratti, Bonnie J. Clark, Roger N. Nicholson, Phil D. TI Global circulation as the main source of cloud activity on Titan SO NATURE LA English DT Article ID TROPOSPHERIC CLOUDS; MIDLATITUDE CLOUDS; METHANE CYCLE; SOUTH-POLE; CASSINI/VIMS; SATURN AB Clouds on Titan result from the condensation of methane and ethane and, as on other planets, are primarily structured by circulation of the atmosphere(1-4). At present, cloud activity mainly occurs in the southern (summer) hemisphere, arising near the pole(5-12) and at mid-latitudes(7,8,13-15) from cumulus updrafts triggered by surface heating and/or local methane sources, and at the north (winter) pole(16,17), resulting from the subsidence and condensation of ethane-rich air into the colder troposphere. General circulation models(1-3) predict that this distribution should change with the seasons on a 15-year timescale, and that clouds should develop under certain circumstances at temperate latitudes (similar to 40 degrees) in the winter hemisphere(2). The models, however, have hitherto been poorly constrained and their long-term predictions have not yet been observationally verified. Here we report that the global spatial cloud coverage on Titan is in general agreement with the models, confirming that cloud activity is mainly controlled by the global circulation. The non-detection of clouds at latitude similar to 40 degrees N and the persistence of the southern clouds while the southern summer is ending are, however, both contrary to predictions. This suggests that Titan's equator-to-pole thermal contrast is overestimated in the models and that its atmosphere responds to the seasonal forcing with a greater inertia than expected. C1 [Rodriguez, Sebastien; Le Mouelic, Stephane; Tobie, Gabriel; Sotin, Christophe] Univ Nantes, CNRS, UMR 6112, Lab Planetol & Geodynam, F-44000 Nantes, France. [Rodriguez, Sebastien] Univ Paris 07, CNRS, CEA Saclay,DSM,IRFU,SAp, Lab AIM,UMR 7158, F-91191 Gif Sur Yvette, France. [Rannou, Pascal] Univ Reims, CNRS, Grp Spectrometrie Mol & Atmospher, UMR 6089, F-51687 Reims, France. [Rannou, Pascal] Univ Versailles St Quentin, CNRS, LATMOS, UMR 7620, F-91371 Verrieres Le Buisson, France. [Baines, Kevin H.; Pitman, Karly M.; Sotin, Christophe; Buratti, Bonnie J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Barnes, Jason W.] NASA, Ames Res Ctr MS 244 30, Moffett Field, CA 94035 USA. [Griffith, Caitlin A.; Brown, Robert H.] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA. [Hirtzig, Mathieu] Univ Michigan, PSL, AOSS, Ann Arbor, MI 48109 USA. [Clark, Roger N.] US Geol Survey, Denver Fed Ctr, Denver, CO 80225 USA. [Nicholson, Phil D.] Cornell Univ, Dept Astron, Ithaca, NY 14853 USA. RP Rodriguez, S (reprint author), Univ Nantes, CNRS, UMR 6112, Lab Planetol & Geodynam, 2 Rue Houssiniere, F-44000 Nantes, France. EM sebastien.rodriguez@cea.fr RI Barnes, Jason/B-1284-2009; RANNOU, Pascal/I-9059-2012; Rodriguez, Sebastien/H-5902-2016 OI Barnes, Jason/0000-0002-7755-3530; Rodriguez, Sebastien/0000-0003-1219-0641 FU CNRS; CEA; CNES French; Universities of Paris Diderot and Nantes FX We thank M. E. Brown for discussions that allowed us greatly to improve the quality of this study. This work was performed partly at the Jet Propulsion Laboratory, California Institute of Technology, under contract to the National Aeronautics and Space Administration. K. M. P. and J. W. B. are supported by the NASA Postdoctoral Program, administered by Oak Ridge Associated Universities. Calibrated VIMS data appear courtesy of the VIMS team. We thank the CNRS, CEA and CNES French agencies, as well as the Universities of Paris Diderot and Nantes for their financial support. NR 28 TC 46 Z9 46 U1 2 U2 10 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 0028-0836 J9 NATURE JI Nature PD JUN 4 PY 2009 VL 459 IS 7247 BP 678 EP 682 DI 10.1038/nature08014 PG 5 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 453KF UT WOS:000266608600038 PM 19494910 ER PT J AU Kim, SW Heckel, A Frost, GJ Richter, A Gleason, J Burrows, JP McKeen, S Hsie, EY Granier, C Trainer, M AF Kim, S. -W. Heckel, A. Frost, G. J. Richter, A. Gleason, J. Burrows, J. P. McKeen, S. Hsie, E. -Y. Granier, C. Trainer, M. TI NO2 columns in the western United States observed from space and simulated by a regional chemistry model and their implications for NOx emissions SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID OZONE MONITORING INSTRUMENT; TROPOSPHERIC NO2; ATMOSPHERIC CHEMISTRY; RADIATIVE-TRANSFER; GOME MEASUREMENTS; NITROGEN-DIOXIDE; MECHANISM; RETRIEVALS; LIFETIMES; SCIAMACHY AB There are many isolated sources of NOx emissions across the western United States, including electrical power generation plants and urban areas. In this manuscript, two satellite instruments measuring NO2 vertical columns over these sources and an atmospheric chemical-transport model are used to evaluate bottom-up NOx emission inventories, model assumptions, and satellite retrieval algorithms. We carried out simulations with the Weather Research and Forecasting-Chemistry (WRF-Chem) model for the western U. S. domain during the summer of 2005 using measured power plant NOx emissions. Model NO2 vertical columns are compared with a retrieval of the Scanning Imaging Absorption Spectrometer for Atmospheric Chartography (SCIAMACHY) satellite instrument data by the University of Bremen and retrievals of the Ozone Monitoring Instrument (OMI) data by the U. S. National Aeronautics and Space Administration (NASA) and a modified version of the NASA OMI retrieval produced by the University of Bremen. For areas dominated by power plant NOx emissions, the model NO2 columns serve as a comparison standard for satellite retrievals because emissions are continuously monitored at all large U. S. power plants. An extensive series of sensitivity tests of the assumptions in both the satellite retrievals and the model are carried out over the Four Corners and San Juan power plants, two adjacent facilities in the northwest corner of New Mexico that together represent the largest NOx point source in the United States. Overall, the SCIAMACHY and OMI NO2 columns over western U. S. power plants agree well with model NO2 columns, with differences between the two being within the variability of the model and satellite. In contrast to regions dominated by power plant emissions, model NO2 columns over large urban areas along the U. S. west coast are approximately twice as large as satellite NO2 columns from SCIAMACHY and OMI retrievals. The discrepancies in urban areas are beyond the sensitivity ranges in the model simulations and satellite observations, implying overestimates of these cities' bottom-up NOx emissions, which are dominated by motor vehicles. Taking the uncertainties in the satellite retrievals into account, our study demonstrates that the tropospheric columns of NO2 retrieved from space-based observations of backscattered solar electromagnetic radiation can be used to evaluate and improve bottom-up emission inventories. C1 [Kim, S. -W.; Frost, G. J.; McKeen, S.; Hsie, E. -Y.; Granier, C.; Trainer, M.] NOAA, Div Chem Sci, Earth Syst Res Lab, Boulder, CO 80305 USA. [Burrows, J. P.] Ctr Ecol & Hydrol, Wallingford OX10 8BB, Oxon, England. [Gleason, J.] NASA, Goddard Space Flight Ctr, Atmospheres Lab, Greenbelt, MD 20771 USA. [Heckel, A.] Swansea Univ, Dept Geog, Swansea SA2 8PP, W Glam, Wales. [Heckel, A.; Richter, A.; Burrows, J. P.] Univ Bremen, Inst Environm Phys, D-28334 Bremen, Germany. [Heckel, A.; Richter, A.; Burrows, J. P.] Univ Bremen, Inst Remote Sensing, D-28334 Bremen, Germany. [Kim, S. -W.; Frost, G. J.; McKeen, S.; Hsie, E. -Y.; Granier, C.] Univ Colorado, Cooperat Inst Res Environm Sci, Boulder, CO 80309 USA. [Granier, C.] Univ Paris 06, UMR7620, Paris, France. [Granier, C.] CNRS, UMR7620, Serv Aeron, Paris, France. RP Kim, SW (reprint author), NOAA, Div Chem Sci, Earth Syst Res Lab, 325 Broadway,R-CSD4, Boulder, CO 80305 USA. EM siwan.kim@noaa.gov RI Richter, Andreas/C-4971-2008; Granier, Claire/D-5360-2013; Trainer, Michael/H-5168-2013; McKeen, Stuart/H-9516-2013; Frost, Gregory/I-1958-2013; Kim, Si-Wan/I-3979-2013; Hsie, Eirh-Yu/I-4449-2013; Burrows, John/B-6199-2014; Manager, CSD Publications/B-2789-2015 OI Richter, Andreas/0000-0003-3339-212X; Granier, Claire/0000-0001-7344-7995; Kim, Si-Wan/0000-0002-7889-189X; Hsie, Eirh-Yu/0000-0003-3934-9923; Burrows, John/0000-0002-6821-5580; FU University of Bremen; European Union; NOAA's Health of the Atmosphere research program FX Many thanks go to G. Grell, S. Peckham, M. Salzmann, B. Skamarock, and R. Portmann for numerous discussions about the WRF-Chem model. The authors thank R. Harley for assistance with the emission trends analysis. Parts of the satellite retrievals used in this study were funded by the University of Bremen and the European Union through the ACCENT project. The Dutch-Finnish built OMI is part of the NASA EOS Aura satellite payload. The OMI project is managed by NIVR and KNMI in the Netherlands. The authors wish to acknowledge support from NOAA's Health of the Atmosphere research program. NR 67 TC 67 Z9 67 U1 1 U2 27 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X EI 2169-8996 J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD JUN 3 PY 2009 VL 114 AR D11301 DI 10.1029/2008JD011343 PG 29 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 455FA UT WOS:000266742300003 ER PT J AU Zeilhofer, C Schmidt, M Bilitza, D Shum, CK AF Zeilhofer, C. Schmidt, M. Bilitza, D. Shum, C. K. TI Regional 4-D modeling of the ionospheric electron density from satellite data and IRI SO ADVANCES IN SPACE RESEARCH LA English DT Article DE Electron density; B-spline modeling; GNSS; Geometry-free observations ID COMPUTER-GRAPHICS; WAVELETS; PRIMER AB Accurate knowledge of the electron density is the key point in correcting ionospheric delays of electromagnetic measurements and in studying ionosphere physics. During the last decade Global Navigation Satellite Systems (GNSS) have become a promising tool for monitoring ionospheric parameters such as the total electron content (TEC). In this contribution we present a four-dimensional (4-D) model of the electron density consisting of a given reference part, i.e., the International Reference Ionosphere (IRI), and an unknown correction term expanded in terms of multi-dimensional base functions. The corresponding series coefficients are calculable from the satellite measurements by applying parameter estimation procedures. Since satellite data are usually sampled between GPS satellites and ground stations, finer structures of the electron density are modelable just in regions with a sufficient number of ground stations. The proposed method is applied to simulated geometry-free GPS phase measurements. The procedure can be used, for example, to study the equatorial anomaly. (C) 2008 COSPAR. Published by Elsevier Ltd. All rights reserved. C1 [Zeilhofer, C.; Schmidt, M.] DGFI, D-80539 Munich, Germany. [Bilitza, D.] NASA, Goddard Space Flight Ctr, Heliospher Phys Lab, GMU, Greenbelt, MD 20771 USA. [Shum, C. K.] Ohio State Univ, Sch Earth Sci, Columbus, OH 43210 USA. RP Zeilhofer, C (reprint author), DGFI, Alfons Goppel Str 11, D-80539 Munich, Germany. EM zeilhofer@dgfi.badw.de; schmidt@dgfi.badw.de; dieter.bilitza.1@gsfc.nasa.gov; ckshum@osu.edu NR 18 TC 17 Z9 18 U1 0 U2 3 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 0273-1177 J9 ADV SPACE RES JI Adv. Space Res. PD JUN 2 PY 2009 VL 43 IS 11 BP 1669 EP 1675 DI 10.1016/j.asr.2008.09.033 PG 7 WC Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences GA 456LS UT WOS:000266848400011 ER PT J AU Eck, TF Holben, BN Reid, JS Sinyuk, A Hyer, EJ O'Neill, NT Shaw, GE Castle, JRV Chapin, FS Dubovik, O Smirnov, A Vermote, E Schafer, JS Giles, D Slutsker, I Sorokine, M Newcomb, WW AF Eck, T. F. Holben, B. N. Reid, J. S. Sinyuk, A. Hyer, E. J. O'Neill, N. T. Shaw, G. E. Castle, J. R. Vande Chapin, F. S. Dubovik, O. Smirnov, A. Vermote, E. Schafer, J. S. Giles, D. Slutsker, I. Sorokine, M. Newcomb, W. W. TI Optical properties of boreal region biomass burning aerosols in central Alaska and seasonal variation of aerosol optical depth at an Arctic coastal site SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID SKY RADIANCE MEASUREMENTS; SINGLE SCATTERING ALBEDO; WAVELENGTH DEPENDENCE; PHYSICAL-PROPERTIES; ABSORPTION; PARTICLES; VARIABILITY; AERONET; SMOKE; CAMPAIGN AB Long-term monitoring of aerosol optical properties at a boreal forest AERONET site in interior Alaska was performed from 1994 through 2008 (excluding winter). Large interannual variability was observed, with some years showing near background aerosol optical depth (AOD) levels (<0.1 at 500 nm) while 2004 and 2005 had August monthly means similar in magnitude to peak months at major tropical biomass burning regions. Single scattering albedo (omega(0); 440 nm) at the boreal forest site ranged from similar to 0.91 to 0.99 with an average of similar to 0.96 for observations in 2004 and 2005. This suggests a significant amount of smoldering combustion of woody fuels and peat/soil layers that would result in relatively low black carbon mass fractions for smoke particles. The fine mode particle volume median radius during the heavy burning years was quite large, averaging similar to 0.17 mu m at AOD(440 nm) = 0.1 and increasing to similar to 0.25 mu m at AOD(440 nm) = 3.0. This large particle size for biomass burning aerosols results in a greater relative scattering component of extinction and, therefore, also contributes to higher omega(0). Additionally, monitoring at an Arctic Ocean coastal site (Barrow, Alaska) suggested transport of smoke to the Arctic in summer resulting in individual events with much higher AOD than that occurring during typical spring Arctic haze. However, the springtime mean AOD(500 nm) is higher during late March through late May (similar to 0.150) than during summer months (similar to 0.085) at Barrow partly due to very few days with low background AOD levels in spring compared with many days with clean background conditions in summer. C1 [Eck, T. F.; Holben, B. N.; Sinyuk, A.; Smirnov, A.; Schafer, J. S.; Giles, D.; Slutsker, I.; Sorokine, M.; Newcomb, W. W.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Eck, T. F.] Univ Maryland, Goddard Earth Sci & Technol Ctr, Baltimore, MD 21201 USA. [Reid, J. S.; Hyer, E. J.] USN, Aerosol & Radiat Sect, Marine Meteorol Div, Res Lab, Monterey, CA 93943 USA. [Sinyuk, A.; Smirnov, A.; Schafer, J. S.; Giles, D.; Slutsker, I.; Sorokine, M.; Newcomb, W. W.] Sci Syst & Applicat Inc, Lanham, MD USA. [O'Neill, N. T.] Univ Sherbrooke, CARTEL, Dept Geomat Appl, Sherbrooke, PQ J1K 2R1, Canada. [Shaw, G. E.] Univ Alaska, Inst Geophys, Fairbanks, AK 99775 USA. [Castle, J. R. Vande] Univ New Mexico, Dept Biol, Albuquerque, NM 87131 USA. [Chapin, F. S.] Univ Alaska, Inst Arct Biol, Fairbanks, AK 99775 USA. [Dubovik, O.] Univ Lille, CNRS, Opt Atmospher Lab, Villeneuve Dascq, France. [Vermote, E.] Univ Maryland, Dept Geog, College Pk, MD 20742 USA. RP Eck, TF (reprint author), NASA, Goddard Space Flight Ctr, Code 614-4, Greenbelt, MD 20771 USA. EM thomas.f.eck@nasa.gov RI Smirnov, Alexander/C-2121-2009; Schafer, Joel/A-3978-2010; ECK, THOMAS/D-7407-2012; Vermote, Eric/K-3733-2012; Dubovik, Oleg/A-8235-2009; Reid, Jeffrey/B-7633-2014; Hyer, Edward/E-7734-2011; OI Smirnov, Alexander/0000-0002-8208-1304; Dubovik, Oleg/0000-0003-3482-6460; Reid, Jeffrey/0000-0002-5147-7955; Hyer, Edward/0000-0001-8636-2026; Chapin III, F Stuart/0000-0002-2558-9910 FU NASA EOS project office; Radiation Sciences Program, NASA Headquarters; NASA Interdisciplinary Science Program; Office of Naval Research Code 32 FX This project was supported by Michael D. King, retired in 2008 from the NASA EOS project office, and by Hal B. Maring, Radiation Sciences Program, NASA Headquarters. We thank the site managers at the Bonanza Creek site (currently Jamie Hollingsworth, University of Alaska Fairbanks) and the Barrow site (currently Walter Brower and Jimmy Ivanoff) for their diligence over the years in operating and maintaining the AERONET instrumentation. Bernie Zak was the coordinator and Rick Wagener was the principal investigator for the Barrow AERONET site. Drs. Reid and Hyer's participation was funded by the NASA Interdisciplinary Science Program and the Office of Naval Research Code 32. We also thank the anonymous reviewers for comments that resulted in improvements in the manuscript. This paper is dedicated to the memory of Wayne Newcomb (1952-2008) of the NASA AERONET project, whose ability to keep AERONET sites working through his combination of extensive knowledge, timely communication, and good humor will never be forgotten. NR 55 TC 63 Z9 63 U1 1 U2 12 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 JUN 2 PY 2009 VL 114 AR D11201 DI 10.1029/2008JD010870 PG 14 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 455EZ UT WOS:000266742200004 ER PT J AU Lu, X Liu, AZ Swenson, GR Li, T Leblanc, T McDermid, IS AF Lu, Xian Liu, Alan Z. Swenson, Gary R. Li, Tao Leblanc, Thierry McDermid, I. Stuart TI Gravity wave propagation and dissipation from the stratosphere to the lower thermosphere SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID STARFIRE OPTICAL-RANGE; ATMOSPHERIC THERMAL TIDES; RESOLUTION DOPPLER IMAGER; LIDAR OBSERVATIONS; MIDDLE ATMOSPHERE; MESOPAUSE REGION; RAYLEIGH LIDAR; VERTICAL STRUCTURE; STABILITY ANALYSIS; TEMPERATURE AB One-night (28 October 2003) temperature and horizontal wind measurements by a resonance sodium (Na) wind/temperature lidar at Maui (20.7 degrees N, 156.3 degrees W) and temperature measurement by a Rayleigh lidar at Mauna Loa Observatory (MLO, 19.5 degrees N, 155.6 degrees W), Hawaii, were used to study gravity wave (GW) propagation from the lower stratosphere to the lower thermosphere. A dominant wave mode was identified from 35 to 103 km. The wave was partially dissipated and propagating upward with a scale height of temperature amplitude at similar to 14 km. A damping layer was present around the stratopause where the wave amplitude was small, which also corresponded to a low static stability layer. The vertical wavelengths were larger in the mesosphere (12-13 km) than in the stratosphere (6-7 km), consistent with the decreasing static stability with altitude. Hodograph analysis of the Na lidar wind data showed that the wave was propagating northward and the horizontal wavelength was 2140 km and intrinsic period was 15 h in the region 84-103 km. The apparent period was similar to 6 h and consistent with Doppler shift of the background wind. It is suggested that the convective zone over the equator to the south of Hawaii provided a constant GW source that is responsible for the observed GW throughout the night. C1 [Lu, Xian] Univ Illinois, Dept Atmospher Sci, Urbana, IL 61801 USA. [Leblanc, Thierry; McDermid, I. Stuart] CALTECH, Jet Prop Lab, Table Mt Facil, Wrightwood, CA 92397 USA. [Li, Tao] Univ Sci & Technol China, Sch Earth & Space Sci, Hefei 230026, Anhui, Peoples R China. [Liu, Alan Z.; Swenson, Gary R.] Univ Illinois, Dept Elect & Comp Engn, Urbana, IL 61801 USA. RP Lu, X (reprint author), Univ Illinois, Dept Atmospher Sci, 105 S Gregory Ave, Urbana, IL 61801 USA. EM xianlu2@uiuc.edu RI Li, Tao/J-8950-2014; Lu, Xian/A-2980-2015; Liu, Alan/C-3738-2008 OI Li, Tao/0000-0002-5100-4429; Lu, Xian/0000-0002-2535-8151; Liu, Alan/0000-0002-1834-7120 FU NSF [ATM 05-45704]; lidar consortium; [ATM 07-37656] FX We would like to thank NASA Jet Propulsion Laboratory (California Institute of Technology) for providing the Rayleigh lidar observation. This study is sponsored by NSF grants ATM 05-45704, the lidar consortium grant, and ATM 07-37656. NR 59 TC 25 Z9 26 U1 2 U2 8 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 JUN 2 PY 2009 VL 114 AR D11101 DI 10.1029/2008JD010112 PG 13 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 455EZ UT WOS:000266742200001 ER PT J AU Stahl, HP Sumrall, P Hopkins, R AF Stahl, H. Philip Sumrall, Phil Hopkins, Randall TI Ares V launch vehicle: An enabling capability for future space science missions SO ACTA ASTRONAUTICA LA English DT Article DE Ares V launch vehicle; Space science; Planetary science; Astrophysics; Large space telescopes AB NASA's planned Ares V cargo launch vehicle offers the potential to completely change the paradigm of future space science mission architectures. Future space science telescopes desire increasingly larger telescope collecting aperture. But, current launch vehicle mass and volume constraints are a severe limit. The Ares V greatly relaxes these constraints. For example, while current launch vehicles have the ability to place a 4.5 m diameter payload with a mass of 9400 kg on to a Sun-Earth L2 transfer trajectory, the Ares V is projected to have the ability to place an 8.8m diameter payload with a mass of approximately 60,000kg on to the same trajectory, or 180,000kg into Low Earth Orbit. Also the Ares V could place approximately 3000kg (13,000kg with a Centaur upper stage) on to a trajectory with a C3 of 106km(2)/s(2), arriving at Saturn in 6.1 years without the use of gravity assists. This paper summarizes the current planned Ares V payload launch capability. Published by Elsevier Ltd. C1 [Stahl, H. Philip; Sumrall, Phil; Hopkins, Randall] NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA. RP Stahl, HP (reprint author), NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA. EM h.philip.stahl@nasa.gov NR 18 TC 6 Z9 6 U1 0 U2 3 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0094-5765 J9 ACTA ASTRONAUT JI Acta Astronaut. PD JUN-JUL PY 2009 VL 64 IS 11-12 BP 1032 EP 1040 DI 10.1016/j.actaastro.2008.12.017 PG 9 WC Engineering, Aerospace SC Engineering GA 440XB UT WOS:000265731900003 ER PT J AU Cha, SS Ramachandran, N Worek, WM AF Cha, Soyoung S. Ramachandran, Narayanan Worek, William M. TI Heat transfer of thermocapillary convection in a two-layered fluid system under the influence of magnetic field SO ACTA ASTRONAUTICA LA English DT Article ID IMMISCIBLE LIQUID LAYERS; MARANGONI CONVECTION; NATURAL-CONVECTION; FREE-SURFACE; BUOYANCY; FLOW AB Heat transfer of a two-layer fluid system has been of great importance in a variety of industrial applications. For example, the phenomena of immiscible fluids can be found in materials processing and heat exchangers. Typically in solidification from a melt, the convective motion is the dominant factor that affects the uniformity of material properties. In the layered flow, thermocapillary forces can come into an important play, which was first emphasized by a previous investigator in 1958. Under extraterrestrial environments without gravity, thermocapillary effects can be a more dominant factor, which alters material properties in processing. Control and optimization of heat transfer in an immiscible fluid system need complete understanding of the flow phenomena that can be induced by surface tension at a fluid interface. The present work is focused on understanding of the magnetic field effects on thermocapillary convection, in order to optimize material processing. That is, it involves the study of the complicated phenomena to alter the flow motion in crystal growth. In this effort, the Marangoni convection in a cavity with differentially heated sidewalls is investigated with and without the influence of a magnetic field. As a first step, numerical analyzes are performed, by thoroughly investigating influences of all pertinent physical parameters. Experiments are then conducted, with preliminary results, for comparison with the numerical analyzes. (C) 2009 Elsevier Ltd. All fights reserved. C1 [Cha, Soyoung S.; Worek, William M.] Univ Illinois, Chicago, IL 60607 USA. [Ramachandran, Narayanan] NASA, George C Marshall Space Flight Ctr, Jacobs ESTS Grp, Huntsville, AL 35812 USA. RP Cha, SS (reprint author), Univ Illinois, Chicago, IL 60607 USA. EM sscha@uic.edu; narayanan.ramachandran-1@nasa.gov; wworek@uic.edu RI Chen, Hongyin/J-2955-2013 OI Chen, Hongyin/0000-0002-2534-0285 NR 18 TC 1 Z9 2 U1 0 U2 0 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0094-5765 J9 ACTA ASTRONAUT JI Acta Astronaut. PD JUN-JUL PY 2009 VL 64 IS 11-12 BP 1066 EP 1079 DI 10.1016/j.actaastro.2009.01.018 PG 14 WC Engineering, Aerospace SC Engineering GA 440XB UT WOS:000265731900006 ER PT J AU Krishen, K AF Krishen, Kumar TI Space applications for ionic polymer-metal composite sensors, actuators, and artificial muscles SO ACTA ASTRONAUTICA LA English DT Article ID BIOMIMETIC SENSORS; SPACEFLIGHT AB Ionic polymer-metal composites (IPMCs) are composites of a noble metal, conductive polymer or carbon/graphite, and charged polyelectrolyte membrane. IPMCs have shown considerable progress in producing actuation in electric fields. These composites are also capable of sensing motion by producing a voltage difference when bent by a mechanical force. Work to date has yielded a force greater than 40 times the weight of an IPMC and large bending displacements with very low-input voltages. There is sufficient reason to believe that artificial muscles with viable strength can be produced with these composites. The IPMC, in addition to being resilient and elastic, is also lightweight and has a reaction speed that ranges from I microsecond to I second. For space missions, devices based on IPMCs will have numerous applications. On planetary surfaces, robotic arms and end effectors, motion-producing motors, actuators, and controllers are just a few examples of devices that can be produced using IPMCs. In this paper, examples of various envisioned space applications of IPMCs will be provided. The impacts of these applications on future space missions will also be discussed. Published by Elsevier Ltd. C1 NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. RP Krishen, K (reprint author), NASA, Lyndon B Johnson Space Ctr, 2102 Nasa Pkwy, Houston, TX 77058 USA. EM kumar.krishen-1@nasa.gov NR 21 TC 33 Z9 37 U1 1 U2 8 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0094-5765 J9 ACTA ASTRONAUT JI Acta Astronaut. PD JUN-JUL PY 2009 VL 64 IS 11-12 BP 1160 EP 1166 DI 10.1016/j.actaastro.2009.01.008 PG 7 WC Engineering, Aerospace SC Engineering GA 440XB UT WOS:000265731900013 ER PT J AU Arcioni, M Daehler, E Mueller, RP van der Meulen, W AF Arcioni, Marco Daehler, Erik Mueller, Robert P. van der Meulen, Wencke TI S@tMax-A space-based system enabling mobile IP applications in vehicles SO ACTA ASTRONAUTICA LA English DT Article AB As personal mobility increases, people spend more time in their vehicles. Furthermore, a large segment of today's workforce is part of a growing mobile service industry. This mobile society creates opportunities to increase productivity which do not yet exist. Today's commuting time could be better utilized and mobile business transactions could be more efficiently conducted, by integrating mobile IP wireless services in vehicles. By means of a direct to mobile user Internet access, and total IP services, integrated into automobiles, S@tMax services can empower the mobile business movement therefore improving productivity. This paper presents a commercial system architecture that will deliver an optimized solution for direct to mobile user Internet access, through an integration of a ground based network infrastructure, use of existing communications satellites and the development of a proprietary satellite system. As a result of a detailed systems engineering process, the architectures of the space, ground and infrastructures segments will be presented. Furthermore, the benefits of on-orbit servicing were examined in the S@tMax context. The approach proposed is considered as an important step towards enforcing main roadway IP coverage in the US, for near-continuous communications and services. (C) 2009 Elsevier Ltd. All fights reserved. C1 [Arcioni, Marco] European Space Technol Ctr, European Space Agcy, TEC SWM, NL-2200 AG Noordwijk, Netherlands. [Daehler, Erik] Boeing Co, Seal Beach, CA 90740 USA. [Mueller, Robert P.] NASA, MS KT C HI, Kennedy Space Ctr, FL 32899 USA. [van der Meulen, Wencke] Netherlands Agcy Aerosp programmes NIVR, NL-2629 HS Delft, Netherlands. RP Arcioni, M (reprint author), European Space Technol Ctr, European Space Agcy, TEC SWM, Keplerlaan 1, NL-2200 AG Noordwijk, Netherlands. EM marco.arcioni@esa.int; erik.s.daehler@boeing.com; rob.mueller@nasa.gov; w.vandermeulen@nivr.nl NR 10 TC 1 Z9 1 U1 1 U2 1 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0094-5765 J9 ACTA ASTRONAUT JI Acta Astronaut. PD JUN-JUL PY 2009 VL 64 IS 11-12 BP 1167 EP 1179 DI 10.1016/j.actaastro.2009.01.028 PG 13 WC Engineering, Aerospace SC Engineering GA 440XB UT WOS:000265731900014 ER PT J AU Rummel, JD AF Rummel, John D. TI Special regions in Mars exploration: Problems and potential SO ACTA ASTRONAUTICA LA English DT Article AB "Special regions" on Mars are areas designated in the COSPAR planetary protection policy as areas that may support Earth microbes inadvertently introduced to Mars, or that may have a high probability of supporting indigenous martian life. Since absolutely nothing is known about martian life, the operational definition of a special region is a place that may allow the formation and maintenance of liquid water, on or under the surface of Mars. This paper will review the special-regions concept, the implications of recent recommendations on avoiding them, and the work of the Mars science community in providing an operational definition of those areas on Mars that are "non-special." Published by Elsevier Ltd. C1 NASA Headquarters, Sci Mission Directorate, Washington, DC 20546 USA. RP Rummel, JD (reprint author), NASA Headquarters, Sci Mission Directorate, Washington, DC 20546 USA. EM jrummel@hq.nasa.gov NR 5 TC 7 Z9 7 U1 0 U2 6 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0094-5765 J9 ACTA ASTRONAUT JI Acta Astronaut. PD JUN-JUL PY 2009 VL 64 IS 11-12 BP 1293 EP 1297 DI 10.1016/j.actaastro.2009.01.006 PG 5 WC Engineering, Aerospace SC Engineering GA 440XB UT WOS:000265731900022 ER PT J AU Macdougall, FW Jow, TR Ennis, JB Yang, XH Yen, SPS Cooper, RA Gilbert, JE Schneider, M Naruo, C Bates, J AF Macdougall, F. W. Jow, T. R. Ennis, J. B. Yang, X. H. Yen, S. P. S. Cooper, R. A. Gilbert, J. E. Schneider, M. Naruo, C. Bates, J. TI Pulsed Power and Power Conditioning Capacitors SO ACTA PHYSICA POLONICA A LA English DT Article; Proceedings Paper CT 2nd Euro-Asian Pulsed Power Conf/4th European Pulsed Power Symp/7th Int Symp Pulsed Power and Plasma Applicat/5th Pulsed Power Applicat Symp/IET Pulsed Power Symp CY SEP 22-26, 2008 CL Vilnius, LITHUANIA SP Int Soc Pulsed Power Applicat, Semicond Phys Inst Vilnius, German French Res Inst St Louis, Vilnius Gediminas Tech Univ AB A capacitor development effort focused on capacitors used in pulsed power and power conversion applications underwent at General Atomics Electronic Systems Inc. (CA-ESI) for decades. In recent years, funding for these efforts has accelerated the rate of development progress to the point where the time it takes to decrease the size of a capacitor by half has dropped from 10 years to 4 years. This progress made in pulsed power and power conversion capacitors will be described along with the performance characteristics of today's capacitors. C1 [Macdougall, F. W.; Ennis, J. B.; Yang, X. H.; Cooper, R. A.; Gilbert, J. E.; Schneider, M.; Naruo, C.; Bates, J.] Gen Atom Elect Syst Inc, San Diego, CA USA. [Jow, T. R.] USA, Res Lab, Adelphi, MD USA. [Yen, S. P. S.] NASA Jet Prop Lab, Pasadena, CA USA. RP Macdougall, FW (reprint author), Gen Atom Elect Syst Inc, San Diego, CA USA. EM fred.macdougall@ga-esi.com NR 3 TC 1 Z9 1 U1 0 U2 2 PU POLISH ACAD SCIENCES INST PHYSICS PI WARSAW PA AL LOTNIKOW 32-46, PL-02-668 WARSAW, POLAND SN 0587-4246 J9 ACTA PHYS POL A JI Acta Phys. Pol. A PD JUN PY 2009 VL 115 IS 6 BP 989 EP 991 PG 3 WC Physics, Multidisciplinary SC Physics GA 474QK UT WOS:000268298900014 ER PT J AU Morris, RA Gasch, J Khatib, L AF Morris, Robert A. Gasch, John Khatib, Lina TI Local Search for Optimal Global Map Generation Using Middecadal Landsat Images SO AI MAGAZINE LA English DT Article; Proceedings Paper CT Conference on Innovative Applications Artificial Intelligence CY JUL 13-17, 2008 CL Chicago, IL ID CONSTRAINT OPTIMIZATION; VARIABLE ELIMINATION AB NASA and the United States Geological Survey (USGS) arc, collaborating to produce a global map of the Earth using Landsat 5 Thematic Mapper (TM) and Landsat 7 Enhanced Thematic Mapper Plus (ETM+) remote sensor data from tire period of 2004 through 2007. The map is composed of thousands of scene locations, and for each location there are tens of different images of varying quality to choose from. Constraints and preferences on map quality make it desirable to develop an automated solution to the map-generation problem. This article formulates a global map-generator problem as a constraint-optimization problem (GMG-COP) and describes an approach to solving it using local search. The article also describes the integration of a GMG solver into a graphical user interface for visualizing and comparing solutions, thus allowing for solutions to be generated with human participation and guidance. C1 [Morris, Robert A.] NASA, Ames Res Ctr, Intelligent Syst Div, Automated Planning & Scheduling Grp, Washington, DC USA. [Gasch, John] NASA, Goddard Space Flight Ctr, Washington, DC USA. [Khatib, Lina] NASA, Ames Res Ctr, SGT Inc, Washington, DC USA. RP Morris, RA (reprint author), NASA, Ames Res Ctr, Intelligent Syst Div, Automated Planning & Scheduling Grp, Washington, DC USA. NR 8 TC 0 Z9 0 U1 0 U2 1 PU AMER ASSOC ARTIFICIAL INTELL PI MENLO PK PA 445 BURGESS DRIVE, MENLO PK, CA 94025-3496 USA SN 0738-4602 J9 AI MAG JI AI Mag. PD SUM PY 2009 VL 30 IS 2 BP 84 EP 95 PG 12 WC Computer Science, Artificial Intelligence SC Computer Science GA 462IH UT WOS:000267344100007 ER PT J AU Daso, EO Pritchett, VE Wang, TS Ota, DK Blankson, IM Auslender, AH AF Daso, Endwell O. Pritchett, Victor E. Wang, Ten-See Ota, Dale K. Blankson, Isaiah M. Auslender, Aaron H. TI Dynamics of Shock Dispersion and Interactions in Supersonic Freestreams with Counterflowing Jets SO AIAA JOURNAL 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 BODY; INJECTION; BODIES; FLOWS AB This study describes an active flow control concept that uses counterflowing jets to significantly modify external flowfields and strongly disperse the shock waves of supersonic and hypersonic vehicles to reduce aerothermal loads and wave drag. The potential aerothermal and aerodynamic benefits of the concepts were investigated by conducting experiments on a 2.6%-scale Apollo capsule model in Mach 3.48 and 4.0 freestreams in a trisonic blowdown wind tunnel, as well as pretest computational fluid dynamics analyses of the flowfields, with and without counterflowing jets. The model employed three sonic and two supersonic (with design Mach numbers of 2.44 and 2.94) jet nozzles with exit diameters ranging from 0.25 to 0.5 in. The schlieren images were consistent with the pretest computational fluid dynamics predictions, showing a long penetration mode jet interaction at low jet flow rates of 0.05 and 0.1 lb(m)/s, whereas a short penetration mode jet was revealed at higher flow rates. The long penetration mode jet appeared to be almost fully expanded and was unsteady, with the how shock becoming so dispersed that it was no longer discernible. High-speed camera schlieren data revealed the bow shock to be dispersed into striations of compression waves, which suddenly coalesced to a weaker bow shock with a larger standoff distance as the How rate reached a critical value. Heat transfer results showed a significant reduction in heat flux, even giving negative heat flux for some short penetration mode interactions, indicating that the flow wetting the model had a cooling effect, instead of heating, which could significantly impact thermal protection system requirements and design. The findings suggest that high-speed vehicle design and performance can benefit from the application of counterflowing jets as an active flow control. C1 [Daso, Endwell O.; Pritchett, Victor E.; Wang, Ten-See] NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA. [Ota, Dale K.] HyPerComp Inc, Westlake Village, CA 91362 USA. [Blankson, Isaiah M.] NASA, John H Glenn Res Ctr, Lewis Field, Cleveland, OH 44135 USA. [Auslender, Aaron H.] NASA, Langley Res Ctr, Hyperson Airbreathing Prop Branch, Hampton, VA 23681 USA. RP Daso, EO (reprint author), NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA. NR 60 TC 15 Z9 17 U1 4 U2 13 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 JUN PY 2009 VL 47 IS 6 BP 1313 EP 1326 DI 10.2514/1.30084 PG 14 WC Engineering, Aerospace SC Engineering GA 452CZ UT WOS:000266518700001 ER PT J AU Ramos-Izquierdo, L Scott, VS Connelly, J Schmidt, S Mamakos, W Guzek, J Peters, C Liiva, P Rodriguez, M Cavanaugh, J Riris, H AF Ramos-Izquierdo, Luis Scott, V. Stanley, III Connelly, Joseph Schmidt, Stephen Mamakos, William Guzek, Jeffrey Peters, Carlton Liiva, Peter Rodriguez, Michael Cavanaugh, John Riris, Haris TI Optical system design and integration of the Lunar Orbiter Laser Altimeter SO APPLIED OPTICS LA English DT Article AB The Lunar Orbiter Laser Altimeter (LOLA), developed for the 2009 Lunar Reconnaissance Orbiter (LRO) mission, is designed to measure the Moon's topography via laser ranging. A description of the LOLA optical system and its measured optical performance during instrument-level and spacecraft-level integration and testing are presented. (C) 2009 Optical Society of America C1 [Ramos-Izquierdo, Luis; Connelly, Joseph] NASA, Goddard Space Flight Ctr, Opt Branch, Greenbelt, MD 20771 USA. [Scott, V. Stanley, III; Riris, Haris] NASA, Goddard Space Flight Ctr, Laser Remote Sensing Lab, Greenbelt, MD 20771 USA. [Schmidt, Stephen] NASA, Goddard Space Flight Ctr, Electromech Syst Branch, Greenbelt, MD 20771 USA. [Mamakos, William; Guzek, Jeffrey] Design Interface Inc, Finksburg, MD 21048 USA. [Peters, Carlton] NASA, Goddard Space Flight Ctr, Thermal Syst Branch, Greenbelt, MD 20771 USA. [Liiva, Peter; Rodriguez, Michael] Sigma Space Corp, Lanham, MD 20706 USA. [Cavanaugh, John] NASA, Goddard Space Flight Ctr, Laser & Electroopt Branch, Greenbelt, MD 20771 USA. RP Ramos-Izquierdo, L (reprint author), NASA, Goddard Space Flight Ctr, Opt Branch, Greenbelt, MD 20771 USA. EM Luis.A.Ramos-Izquierdo@nasa.gov RI Scott, Vibart/B-5086-2013; Riris, Haris/D-1004-2013 NR 7 TC 8 Z9 8 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 JUN 1 PY 2009 VL 48 IS 16 BP 3035 EP 3049 DI 10.1364/AO.48.003035 PG 15 WC Optics SC Optics GA 460QO UT WOS:000267202400010 PM 19488116 ER PT J AU Kobayashi, NP Mathai, S Li, XM Logeeswaran, VJ Islam, MS Lohn, A Onishi, T Straznicky, J Wang, SY Williams, RS AF Kobayashi, Nobuhiko P. Mathai, Sagi Li, Xuema Logeeswaran, V. J. Islam, M. Saif Lohn, Andrew Onishi, Takehiro Straznicky, Joseph Wang, Shih-Yuan Williams, R. Stanley TI Ensembles of indium phosphide nanowires: physical properties and functional devices integrated on non-single crystal platforms SO APPLIED PHYSICS A-MATERIALS SCIENCE & PROCESSING LA English DT Article ID OPTICAL-PROPERTIES; AMORPHOUS-SILICON; GROWTH; NANONEEDLES; MECHANISMS; SURFACES AB A new route to grow an ensemble of indium phosphide single-crystal semiconductor nanowires is described. Unlike conventional epitaxial growth of single-crystal semiconductor films, the proposed route for growing semiconductor nanowires does not require a single-crystal semiconductor substrate. In the proposed route, instead of using single-crystal semiconductor substrates that are characterized by their long-range atomic ordering, a template layer that possesses short-range atomic ordering prepared on a non-single-crystal substrate is employed. On the template layer, epitaxial information associated with its short-range atomic ordering is available within an area that is comparable to that of a nanowire root. Thus the template layer locally provides epitaxial information required for the growth of semiconductor nanowires. In the particular demonstration described in this paper, hydrogenated silicon was used as a template layer for epitaxial growth of indium phosphide nanowires. The indium phosphide nanowires grown on the hydrogenerated silicon template layer were found to be single crystal and optically active. Simple photoconductors and pin-diodes were fabricated and tested with the view towards various optoelectronic device applications where group III-V compound semiconductors are functionally integrated onto non-single-crystal platforms. C1 [Kobayashi, Nobuhiko P.; Lohn, Andrew; Onishi, Takehiro] Univ Calif Santa Cruz, Baskin Sch Engn, Santa Cruz, CA 95064 USA. [Kobayashi, Nobuhiko P.; Lohn, Andrew; Onishi, Takehiro] Univ Calif Santa Cruz, NECTAR, Adv Studies Labs, NASA,Ames Res Ctr, Moffett Field, CA 94035 USA. [Mathai, Sagi; Li, Xuema; Straznicky, Joseph; Wang, Shih-Yuan; Williams, R. Stanley] Hewlett Packard Labs, Informat & Quantum Syst Lab, Palo Alto, CA 94034 USA. [Logeeswaran, V. J.; Islam, M. Saif] Univ Calif Davis, Davis, CA 95616 USA. RP Kobayashi, NP (reprint author), Univ Calif Santa Cruz, Baskin Sch Engn, Santa Cruz, CA 95064 USA. EM nobby@soe.ucsc.edu RI Wang, Shih-Yuan/C-3889-2009; Williams, R. Stanley/A-8281-2009; Kobayashi, Nobuhiko/E-3834-2012 OI Wang, Shih-Yuan/0000-0002-1212-3484; Williams, R. Stanley/0000-0003-0213-4259; NR 32 TC 11 Z9 11 U1 0 U2 6 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0947-8396 J9 APPL PHYS A-MATER JI Appl. Phys. A-Mater. Sci. Process. PD JUN PY 2009 VL 95 IS 4 BP 1005 EP 1013 DI 10.1007/s00339-009-5110-9 PG 9 WC Materials Science, Multidisciplinary; Physics, Applied SC Materials Science; Physics GA 445SW UT WOS:000266072800010 ER PT J AU Baldridge, AM Christensen, PR AF Baldridge, A. M. Christensen, P. R. TI A Laboratory Technique for Thermal Emission Measurement of Hydrated Minerals SO APPLIED SPECTROSCOPY LA English DT Article DE Thermal infrared spectroscopy; Emission spectroscopy; Hydrous minerals; Remote sensing; Mars; Water ID INFRARED-EMISSION; OPTICAL-CONSTANTS; SPECTRAL CONTRAST; PARTICULATE SURFACES; HYDROUS MINERALS; MARTIAN SURFACE; PARTICLE-SIZE; MARS ODYSSEY; MU-M; SPECTROSCOPY AB Laboratory emission spectra are measured at Arizona State University's Mars Space Flight Facility for comparison to remotely sensed data from Earth and Mars. Such emission spectroscopy using an interferometric spectrometer measures the energy of the sample, including reflected and emitted background sources. The detector is uncooled at ambient temperature, which produces a very low signal when measuring the energy from a sample that has a temperature close to its own. In order to increase the energy difference between the sample and the detector, thereby increasing the signal received by the detector, samples are typically heated to between 60 and 80 degrees C for several hours prior to measurement. While this method is acceptable for most rock and mineral samples, some hydrous minerals dehydrate quickly at low relative humidity and temperatures above room temperature. This change is evident in both the physical appearance of the mineral and in the position and shape of its spectral absorptions. One solution to this problem is to heat samples to lower temperatures (e.g., 40 degrees C) for only a short time period. However, this approach results in a low signal from the sample and does not always avoid dehydration. For this reason, we have developed a technique for measuring and calibrating emission spectra of hydrated minerals that involves cooling samples to well below the temperature of the detector, which avoids dehydration, while creating a large delta temperature and a strong signal from the sample. Our method allows for accurate library spectra, with discrete, pronounced spectral features (high spectral contrast), of hydrated minerals that can be used for comparison to planetary surfaces. C1 [Baldridge, A. M.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Christensen, P. R.] Arizona State Univ, Tempe, AZ 85287 USA. RP Baldridge, AM (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM alice.m.baldridge@jpl.nasa.gov NR 51 TC 4 Z9 4 U1 0 U2 10 PU SOC APPLIED SPECTROSCOPY PI FREDERICK PA 5320 SPECTRUM DRIVE SUITE C, FREDERICK, MD 21703 USA SN 0003-7028 EI 1943-3530 J9 APPL SPECTROSC JI Appl. Spectrosc. PD JUN PY 2009 VL 63 IS 6 BP 678 EP 688 PG 11 WC Instruments & Instrumentation; Spectroscopy SC Instruments & Instrumentation; Spectroscopy GA 458SH UT WOS:000267043300011 PM 19531295 ER PT J AU Sun, HJ Saccomanno, V Hedlund, B Mckay, CP AF Sun, Henry J. Saccomanno, Vienna Hedlund, Brian McKay, Christopher P. TI Stereo-Specific Glucose Consumption May Be Used to Distinguish Between Chemical and Biological Reactivity on Mars: A Preliminary Test on Earth SO ASTROBIOLOGY LA English DT Article DE Biosignatures; Life detection; Mars; Microbe ID AMINO-ACIDS; LIFE DETECTION; SOIL; PEPTIDOGLYCANS; DEGRADATION; ATLANTIC; SEAWATER; NITROGEN; DESERT AB Two alternative hypotheses explain the degradation of organics in the Viking Labeled Release experiment on Mars. Either martian soil contains live indigenous microorganisms or it is sterile but chemically reactive. These two possibilities could be distinguished by the use of pure preparations of glucose isomers. In the laboratory, selected eukaryotes, bacteria, and archaea consumed only D-glucose, not L-glucose, while permanganate oxidized both isomers. On Mars, selective consumption of either D- or L-glucose would constitute evidence for biological activity. C1 [Sun, Henry J.; Saccomanno, Vienna] Desert Res Inst, Div Earth & Ecosyst Sci, Las Vegas, NV 89119 USA. [Hedlund, Brian] Univ Nevada, Sch Life Sci, Las Vegas, NV 89154 USA. [McKay, Christopher P.] NASA, Ames Res Ctr, Div Space Sci, Moffett Field, CA 94035 USA. RP Sun, HJ (reprint author), Desert Res Inst, Div Earth & Ecosyst Sci, Las Vegas, NV 89119 USA. EM henry.sun@dri.edu FU NASA EPSCoR [NNX07AT65]; NASA [NNX08AO45G] FX This work was supported by a NASA EPSCoR grant to Nevada (NNX07AT65) and a NASA grant to H.J. Sun (NNX08AO45G). NR 26 TC 11 Z9 11 U1 0 U2 4 PU MARY ANN LIEBERT INC PI NEW ROCHELLE PA 140 HUGUENOT STREET, 3RD FL, NEW ROCHELLE, NY 10801 USA SN 1531-1074 J9 ASTROBIOLOGY JI Astrobiology PD JUN PY 2009 VL 9 IS 5 BP 443 EP 446 DI 10.1089/ast.2008.0315 PG 4 WC Astronomy & Astrophysics; Biology; Geosciences, Multidisciplinary SC Astronomy & Astrophysics; Life Sciences & Biomedicine - Other Topics; Geology GA 464TB UT WOS:000267528700002 PM 19566424 ER PT J AU DeWitt, HL Trainer, MG Pavlov, AA Hasenkopf, CA Aiken, AC Jimenez, JL McKay, CP Toon, OB Tolbert, MA AF DeWitt, H. Langley Trainer, Melissa G. Pavlov, Alex A. Hasenkopf, Christa A. Aiken, Allison C. Jimenez, Jose L. McKay, Christopher P. Toon, Owen B. Tolbert, Margaret A. TI Reduction in Haze Formation Rate on Prebiotic Earth in the Presence of Hydrogen SO ASTROBIOLOGY LA English DT Article DE Atmosphere; Atmospheric compositions; Carbon dioxide; Early Earth ID AEROSOL MASS-SPECTROMETER; ATMOSPHERE; CHEMISTRY; TITAN AB Recent attempts to resolve the faint young Sun paradox have focused on an early Earth atmosphere with elevated levels of the greenhouse gases methane (CH4) and carbon dioxide (CO2) that could have provided adequate warming to Earth's surface. On Titan, the photolysis of CH4 has been shown to create a thick haze layer that cools its surface. Unlike Titan, however, early Earth's atmosphere likely contained high amounts of CO2 and hydrogen (H-2). In this work, we examine haze formation in an early Earth atmosphere composed of CO2, H-2, N-2, and CH4, with a CO2/CH4 ratio of 10 and a H-2/CO2 ratio of up to 15. To initiate aerosol formation, a broad-spectrum ultraviolet (UV) energy source with emission at Lyman-alpha was used to simulate the solar spectrum. Aerosol composition and total aerosol mass produced as a function of reagent gas were measured with an aerosol mass spectrometer (AMS). Results show an order of magnitude decrease in haze production with the addition of H-2, with no significant change in the chemical composition of the haze. We calculate that the presence of H-2 on early Earth could thus have favored warmer surface temperatures and yet allowed photochemical haze formation to deliver complex organic species to early Earth's surface. C1 [DeWitt, H. Langley; Aiken, Allison C.; Jimenez, Jose L.; Tolbert, Margaret A.] Univ Colorado, Dept Chem & Biochem, Boulder, CO 80302 USA. [DeWitt, H. Langley; Trainer, Melissa G.; Hasenkopf, Christa A.; Aiken, Allison C.; Jimenez, Jose L.; Tolbert, Margaret A.] Univ Colorado, Cooperat Inst Res Environm Sci, Boulder, CO 80302 USA. [Pavlov, Alex A.] Univ Arizona, Dept Planetary Sci, Lunar & Planetary Lab, Tucson, AZ 85721 USA. [Trainer, Melissa G.; Toon, Owen B.] Dept Atmospher & Ocean Sci, Boulder, CO USA. [Trainer, Melissa G.; Toon, Owen B.] Univ Colorado, Atmospher & Space Phys Lab, Boulder, CO 80309 USA. [McKay, Christopher P.] NASA, Ames Res Ctr, Div Space Sci, Moffett Field, CA 94035 USA. RP DeWitt, HL (reprint author), Univ Colorado, Dept Chem & Biochem, UCB 216, Boulder, CO 80302 USA. EM dewitt@colorado.edu RI Jimenez, Jose/A-5294-2008; Aiken, Allison/B-9659-2009; Trainer, Melissa/E-1477-2012 OI Jimenez, Jose/0000-0001-6203-1847; Aiken, Allison/0000-0001-5749-7626; FU National Aeronautics and Space Administration ( NASA) [NNGO4GM42G, NNX07AF190, NNX07AV55G]; University of Colorado Center for Astrobiology; Oak Ridge Associated Universities; National Science Foundation FX This material is based on work supported by the National Aeronautics and Space Administration ( NASA) Grants NNGO4GM42G, NNX07AF190, and NNX07AV55G issued through the Office of Space Science. H. Langley DeWitt is supported through a NASA GSRP fellowship. Melissa G. Trainer was supported by an appointment to the NASA Postdoctoral Program at the University of Colorado Center for Astrobiology, administered by Oak Ridge Associated Universities. Christa A. Hasenkopf was supported with a National Science Foundation fellowship. NR 20 TC 19 Z9 19 U1 1 U2 5 PU MARY ANN LIEBERT, INC PI NEW ROCHELLE PA 140 HUGUENOT STREET, 3RD FL, NEW ROCHELLE, NY 10801 USA SN 1531-1074 EI 1557-8070 J9 ASTROBIOLOGY JI Astrobiology PD JUN PY 2009 VL 9 IS 5 BP 447 EP 453 DI 10.1089/ast.2008.0289 PG 7 WC Astronomy & Astrophysics; Biology; Geosciences, Multidisciplinary SC Astronomy & Astrophysics; Life Sciences & Biomedicine - Other Topics; Geology GA 464TB UT WOS:000267528700003 PM 19566425 ER PT J AU Eigenbrode, J Benning, LG Maule, J Wainwright, N Steele, A Amundsen, HEF AF Eigenbrode, Jennifer Benning, Liane G. Maule, Jake Wainwright, Norm Steele, Andrew Amundsen, Hans E. F. CA AMASE 2006 Team TI A Field-Based Cleaning Protocol for Sampling Devices Used in Life-Detection Studies SO ASTROBIOLOGY LA English DT Article DE Organic decontamination; Sterilization; Life detection; Biosignature contaminants; Mars analog; Ice coring ID GLACIER ICE CORE; BACILLUS-SUBTILIS; HYDROGEN-PEROXIDE; LAKE VOSTOK; SPORES; HYPOCHLORITE; SVALBARD; BENEATH; AGENTS; DECONTAMINATION AB Analytical approaches to extant and extinct life detection involve molecular detection often at trace levels. Thus, removal of biological materials and other organic molecules from the surfaces of devices used for sampling is essential for ascertaining meaningful results. Organic decontamination to levels consistent with null values on life-detection instruments is particularly challenging at remote field locations where Mars analog field investigations are carried out. Here, we present a seven-step, multi-reagent decontamination method that can be applied to sampling devices while in the field. In situ lipopolysaccharide detection via low-level endotoxin assays and molecular detection via gas chromatography-mass spectrometry were used to test the effectiveness of the decontamination protocol for sampling of glacial ice with a coring device and for sampling of sediments with a rover scoop during deployment at Arctic Mars-analog sites in Svalbard, Norway. Our results indicate that the protocols and detection technique sufficiently remove and detect low levels of molecular constituents necessary for life-detection tests. C1 [Eigenbrode, Jennifer] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Eigenbrode, Jennifer; Maule, Jake; Steele, Andrew] Carnegie Inst Washington, Geophys Lab, Washington, DC 20015 USA. [Benning, Liane G.] Univ Leeds, Sch Earth & Environm, Earth & Biosphere Inst, Leeds LS2 9JT, W Yorkshire, England. [Wainwright, Norm] Charles River Labs Inc, Charleston, SC USA. [Amundsen, Hans E. F.] Earth & Planetary Explorat, Oslo, Norway. [Maule, Jake] NASA, George C Marshall Space Flight Ctr, Lab On Chip Applicat Dev LOCAD Grp, Huntsville, AL 35812 USA. RP Eigenbrode, J (reprint author), NASA, Goddard Space Flight Ctr, Code 699, Greenbelt, MD 20771 USA. EM Jennifer.Eigenbrode@nasa.gov RI Benning, Liane/E-7071-2011; Eigenbrode, Jennifer/D-4651-2012 OI Benning, Liane/0000-0001-9972-5578; FU Geophysical Laboratory, Carnegie Institution of Washington; University of Leeds; University Centre in Svalbard (UNIS); NASA AMASE-ASTEP; Earth and Biosphere Institute; School of Earth and Environment at the University of Leeds FX We thank the 2005 and 2006 AMASE teams and crew of the Norwegian Polar Institute's R/V Lance for assisting the "cleaning ladies'' during the fieldwork. We are grateful for generous support from the Geophysical Laboratory, Carnegie Institution of Washington, and the University of Leeds. We are indebted to the University Centre in Svalbard (UNIS) for safety training and logistical support, and we thank Charles River Laboratories, Inc., for kindly providing the LAL assay instrumentation and consumables. This work was funded by a NASA AMASE-ASTEP grant led by A. Steele and the Earth and Biosphere Institute and School of Earth and Environment at the University of Leeds, whose financial help made these field seasons possible. NR 45 TC 6 Z9 6 U1 0 U2 6 PU MARY ANN LIEBERT INC PI NEW ROCHELLE PA 140 HUGUENOT STREET, 3RD FL, NEW ROCHELLE, NY 10801 USA SN 1531-1074 J9 ASTROBIOLOGY JI Astrobiology PD JUN PY 2009 VL 9 IS 5 BP 455 EP 465 DI 10.1089/ast.2008.0275 PG 11 WC Astronomy & Astrophysics; Biology; Geosciences, Multidisciplinary SC Astronomy & Astrophysics; Life Sciences & Biomedicine - Other Topics; Geology GA 464TB UT WOS:000267528700004 PM 19496672 ER PT J AU Sun, HJ Saccomanno, V Hedlund, B Mckay, CP AF Sun, Henry J. Saccomanno, Vienna Hedlund, Brian McKay, Christopher P. TI Comment on "Stereo-Specific Glucose Consumption May Be Used to Distinguish Between Chemical and Biological Reactivity on Mars: A Preliminary Test on Earth" Response to Dr. Levin's Comment SO ASTROBIOLOGY LA English DT Editorial Material C1 [Sun, Henry J.; Saccomanno, Vienna] Desert Res Inst, Div Earth & Ecosyst Sci, Las Vegas, NV 89119 USA. [Hedlund, Brian] Univ Nevada, Sch Life Sci, Las Vegas, NV 89154 USA. [McKay, Christopher P.] NASA, Ames Res Ctr, Div Space Sci, Moffett Field, CA 94035 USA. RP Sun, HJ (reprint author), Desert Res Inst, Div Earth & Ecosyst Sci, Las Vegas, NV 89119 USA. EM henry.sun@dri.edu NR 0 TC 0 Z9 0 U1 1 U2 2 PU MARY ANN LIEBERT INC PI NEW ROCHELLE PA 140 HUGUENOT STREET, 3RD FL, NEW ROCHELLE, NY 10801 USA SN 1531-1074 J9 ASTROBIOLOGY JI Astrobiology PD JUN PY 2009 VL 9 IS 5 BP 505 EP 505 DI 10.1089/ast.2009.0395 PG 1 WC Astronomy & Astrophysics; Biology; Geosciences, Multidisciplinary SC Astronomy & Astrophysics; Life Sciences & Biomedicine - Other Topics; Geology GA 464TB UT WOS:000267528700009 ER PT J AU Kelley, MS Wooden, DH Tubiana, C Boehnhardt, H Woodward, CE Harker, DE AF Kelley, Michael S. Wooden, Diane H. Tubiana, Cecilia Boehnhardt, Hermann Woodward, Charles E. Harker, David E. TI SPITZER OBSERVATIONS OF COMET 67P/CHURYUMOV-GERASIMENKO AT 5.5-4.3 AU FROM THE SUN SO ASTRONOMICAL JOURNAL LA English DT Article DE comets: individual (67P/Churyumov-Gerasimenko); infrared: solar system; meteors, meteoroids ID SPACE-TELESCOPE OBSERVATIONS; ROSETTA MISSION; DISTANT COMETS; CCD PHOTOMETRY; SOLAR-SYSTEM; INNER COMA; DUST TRAIL; NUCLEUS; PARTICLES; ENCOUNTER AB We report Spitzer Space Telescope observations of comet 67P/Churyumov-Gerasimenko at 5.5 and 4.3 AU from the Sun, post-aphelion. Comet 67P is the primary target of the European Space Agency's Rosetta mission. The Rosetta spacecraft will rendezvous with the nucleus at heliocentric distances similar to our observations. Rotationally resolved observations at 8 and 24 mu m (at a heliocentric distance, r(h), of 4.8 AU) that sample the size and color-temperature of the nucleus are combined with aphelion R-band light curves observed at the Very Large Telescope (VLT) and yield a mean effective radius of 2.04 +/- 0.11 km, and an R-band geometric albedo of 0.054 +/- 0.006. The amplitudes of the R-band and mid-infrared light curves agree, which suggests that the variability is dominated by the shape of the nucleus. We also detect the dust trail of the comet at 4.8 and 5.5 AU, constrain the grain sizes to be less than or similar to 6 mm, and estimate the impact hazard to Rosetta. We find no evidence for recently ejected dust in our images. If the activity of 67P is consistent from orbit to orbit, then we may expect the Rosetta spacecraft will return images of an inactive or weakly active nucleus as it rendezvous with the comet at r(h) = 4 AU in 2014. C1 [Kelley, Michael S.] Univ Cent Florida, Dept Phys, Orlando, FL 32816 USA. [Wooden, Diane H.] NASA, Ames Res Ctr, Div Space Sci, MS 245 3, Moffett Field, CA 94035 USA. [Tubiana, Cecilia; Boehnhardt, Hermann] Max Planck Inst Solar Syst Res, D-37191 Katlenburg Lindau, Germany. [Woodward, Charles E.] Univ Minnesota, Dept Astron, Minneapolis, MN 55455 USA. [Harker, David E.] Univ Calif San Diego, Ctr Astron & Space Sci, Dept 0424, San Diego, CA 92093 USA. RP Kelley, MS (reprint author), Univ Maryland, Dept Astron, College Pk, MD 20742 USA. EM msk@astro.umd.edu; Diane.H.Wooden@nasa.gov; tubiana@mps.mpg.de; boehnhardt@mps.mpg.de; chelsea@astro.umn.edu; dharker@ucsd.edu OI Harker, David/0000-0001-6397-9082; Kelley, Michael/0000-0002-6702-7676 FU NASA [1289123, 1263741, 1256406, 1215746]; National Science Foundation [AST-0706980] FX The authors acknowledge the Director of the Spitzer Science Center for providing Director's Discretionary Time, and appreciate the hard work of Vikki Meadows and the Observing Support Staff at the SSC for scheduling our rotationally phased light-curve observations, making possible the surface color-temperature measurements. This research made use of Tiny Tim/Spitzer, developed by John Krist for the Spitzer Science Center. This work is based in part on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology under a contract with NASA. Support for this work was provided by NASA through contract 1289123 issued by JPL/Caltech to the University of Central Florida, and contracts 1263741, 1256406, and 1215746 issued by JPL/Caltech to the University of Minnesota. C. E. W. also acknowledges support from the National Science Foundation gran AST-0706980. NR 49 TC 29 Z9 30 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 EI 1538-3881 J9 ASTRON J JI Astron. J. PD JUN PY 2009 VL 137 IS 6 BP 4633 EP 4642 DI 10.1088/0004-6256/137/6/4633 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 454DQ UT WOS:000266662300010 ER PT J AU de Gregorio-Monsalvo, I Gomez, JF Anglada, G Torrelles, JM Kuiper, TBH Suarez, O Patel, NA AF de Gregorio-Monsalvo, Itziar Gomez, Jose F. Anglada, Guillem Torrelles, Jose M. Kuiper, Thomas B. H. Suarez, Olga Patel, Nimesh A. TI RADIO CONTINUUM EMISSION AND WATER MASERS TOWARD CB 54 SO ASTRONOMICAL JOURNAL LA English DT Article DE ISM: globules; ISM: jets and outflows; ISM: molecules; masers; radio continuum: ISM; stars: formation ID YOUNG STELLAR OBJECTS; LOW-MASS STARS; BOK GLOBULES; POWERING SOURCES; NORTHERN SKY; H2O MASERS; OUTFLOWS; REGIONS; PROTOSTARS; AMMONIA AB We present high angular resolution observations of water masers at 1.3 cm and radio continuum emission at 1.3, 3.6, and 6 cm to ward the Bok globule CB 54 using the Very Large Array. At 1.3 cm, with subarcsecond angular resolution, we detect a radio continuum compact source located to the southwest of the globule and spatially coincident with a mid-infrared (mid-IR) embedded object (MIR-b). The spectral index derived between 6 and 1.3 cm (alpha = 0.3 +/- 0.4) is flat, consistent with optically thin free-free emission from ionized gas. We propose the shock-ionization scenario as a viable mechanism for producing the radio continuum emission observed at cm frequencies. Water masers are detected at two different positions separated by 2 ''.3, and coincide spatially with two mid-IR sources: MIR-b and MIR-c. The association of these mid-IR sources with water masers confirms that they are likely protostars undergoing mass loss, and they are the best candidate as driving sources of the molecular outflows in the region. C1 [de Gregorio-Monsalvo, Itziar] European So Observ, Santiago 19, Chile. [Gomez, Jose F.; Anglada, Guillem; Suarez, Olga] CSIC, Inst Astrofis Andalucia, E-18080 Granada, Spain. [Torrelles, Jose M.] Univ Barcelona, Fac Fis, Inst Ciencias Espacio CSIC IEEC, E-08028 Barcelona, Spain. [Kuiper, Thomas B. H.] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. [Suarez, Olga] Univ Nice Sophia Antipolis, CNRS, UMR H Fizeau 6525, F-06108 Nice 2, France. [Patel, Nimesh A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP de Gregorio-Monsalvo, I (reprint author), European So Observ, Alonso Cordova 3107,Casilla 19001, Santiago 19, Chile. RI Gomez, Jose Francisco/D-8392-2016; OI Gomez, Jose Francisco/0000-0002-7065-542X; Torrelles, Jose Maria/0000-0002-6896-6085 FU Ministerio de Ciencia e Innovacion (Spain) [AYA 2008-06189-C03]; Consejeria de Innovacion; Ciencia y Empresa of Junta de Andalucia, (Spain); National Aeronautics and Space Administration; California Institute of Technology FX We thank the referee for providing constructive comments and help in improving the contents of this paper. We are thankful to Per Bergman for his suggestions. G. A., I. d. G., J. F. G., J. M. T., and O. S. are partially supported by Ministerio de Ciencia e Innovacion (Spain), grant AYA 2008-06189-C03 (including FEDER funds), and by Consejeria de Innovacion, Ciencia y Empresa of Junta de Andalucia, (Spain). The work by TBHK was performed in part at the Jet Propulsion Laboratory under contract between the National Aeronautics and Space Administration and the California Institute of Technology. NR 37 TC 1 Z9 1 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 JUN PY 2009 VL 137 IS 6 BP 5080 EP 5085 DI 10.1088/0004-6256/137/6/5080 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 454DQ UT WOS:000266662300045 ER PT J AU Temim, T Gehrz, RD Woodward, CE Roellig, TL Smith, N Rudnick, LR Polomski, EF Davidson, KD Yuen, L Onaka, T AF Temim, Tea Gehrz, Robert D. Woodward, Charles E. Roellig, Thomas L. Smith, Nathan Rudnick, Lawrence R. Polomski, Elisha F. Davidson, Kris D. Yuen, Lunming Onaka, Takashi TI SPITZER SPACE TELESCOPE INFRARED IMAGING AND SPECTROSCOPY OF THE CRAB NEBULA (vol 132, pg 1610, 2006) SO ASTRONOMICAL JOURNAL LA English DT Correction C1 [Temim, Tea; Gehrz, Robert D.; Woodward, Charles E.; Rudnick, Lawrence R.; Polomski, Elisha F.; Davidson, Kris D.] Univ Minnesota, Sch Phys & Astron, Dept Astron, Minneapolis, MN 55455 USA. [Roellig, Thomas L.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Smith, Nathan] Univ Colorado, Ctr Astrophys & Space Astron, Boulder, CO 80309 USA. [Yuen, Lunming] Technosci Corp, Moffett Field, CA 94035 USA. [Onaka, Takashi] Univ Tokyo, Bunkyo Ku, Tokyo 1130033, Japan. RP Temim, T (reprint author), Univ Minnesota, Sch Phys & Astron, Dept Astron, 116 Church St SE, Minneapolis, MN 55455 USA. EM ttemim@astro.umn.edu; gehrz@astro.umn.edu; clwood@astro.umn.edu; Thomas.L.Roellig@nasa.gov; nathans@casa.colorado.edu; larry@astro.umn.edu; kd@astro.umn.edu; lyuen@mail.arc.nasa.gov; onaka@astron.s.u-tokyo.ac.jp RI ONAKA, TAKASHI/G-5058-2014; OI Temim, Tea/0000-0001-7380-3144 NR 4 TC 8 Z9 8 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 JUN PY 2009 VL 137 IS 6 BP 5155 EP 5155 DI 10.1088/0004-6256/137/6/5155 PG 1 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 454DQ UT WOS:000266662300053 ER PT J AU Hirtzig, M Tokano, T Rodriguez, S le Mouelic, S Sotin, C AF Hirtzig, Mathieu Tokano, Tetsuya Rodriguez, Sebastien le Mouelic, Stephane Sotin, Christophe TI A review of Titan's atmospheric phenomena SO ASTRONOMY AND ASTROPHYSICS REVIEW LA English DT Review DE Titan, satellites; Near-infrared; Clouds; Imagery, spectroscopy, spectro-imagery ID HUBBLE-SPACE-TELESCOPE; VOYAGER-1 RADIO-OCCULTATION; NORTH POLAR STRATOSPHERE; ADAPTIVE OPTICS; SEASONAL-CHANGE; TROPOSPHERIC CLOUDS; ZONAL WINDS; MU-M; SPECTROSCOPIC DATABASE; LATITUDINAL TRANSPORT AB Saturn's satellite Titan is a particularly interesting body in our solar system. It is the only satellite with a dense atmosphere, which is primarily made of nitrogen and methane. It harbours an intricate photochemistry, that populates the atmosphere with aerosols, but that should deplete irreversibly the methane. The observation that methane is not depleted led to the study of Titan's methane cycle, starting with its atmospheric part. The features that inhabit Titan's atmosphere can last for timescales varying from year to day. For instance, the reversal of the north-south asymmetry is linked to the 16-year seasonal cycle. Diurnal phenomena have also been observed, like a stratospheric haze enhancement or a possible tropospheric drizzle. Furthermore, clouds have been reported on Titan since 1993. From these first detections and up to now, with the recent inputs from the Cassini-Huygens mission, clouds have displayed a large range of shapes, altitudes, and natures, from the flocky tropospheric clouds at the south pole to the stratiform ones in the northern stratosphere. It is still difficult to compose a clear picture of the physical processes governing these phenomena, even though of lot of different means of observation (spectroscopy, imaging) are available now. We propose here an overview of the phenomena reported between 1993 and 2008 in the low atmosphere of Titan, with indications on the location, altitude, and their characteristics in order to give a perspective of our up-to-date understanding of Titan's meteorological manifestations. We shall focus mainly on direct imaging observations, from both space- and ground-based facilities. All of these observations, published in more than 30 different refereed papers to date, allow us to build a precise chronology of Titan's atmospheric changes (including the north-south asymmetry, diurnal and seasonal effects, etc). Since the interpretation is at an early stage, we only briefly mention some of the current theories regarding the features' nature. C1 [Hirtzig, Mathieu] IPSL, LATMOS, Verrieres Le Buisson, France. [Tokano, Tetsuya] Univ Cologne, Inst Geophys & Meteorol, D-5000 Cologne, Germany. [Rodriguez, Sebastien] Univ Paris Diderot, CNRS, Lab AIM, CEA DSM,IRFU SAp, Gif Sur Yvette, France. [le Mouelic, Stephane] Lab Planetol & Geodynam, Nantes, France. [Sotin, Christophe] CALTECH, Jet Prop Lab, Pasadena, CA USA. RP Hirtzig, M (reprint author), IPSL, LATMOS, Verrieres Le Buisson, France. EM mathieu.hirtzig@aerov.jussieu.fr RI Rodriguez, Sebastien/H-5902-2016 OI Rodriguez, Sebastien/0000-0003-1219-0641 FU DFG FX The authors want to thank Caitlin A. Griffith and Athena Coustenis for fruitful discussions. The constructive comments made by Therese Encrenaz and an anonymous referee were also greatly appreciated. Tetsuya Tokano was supported by DFG. NR 180 TC 12 Z9 12 U1 2 U2 18 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0935-4956 EI 1432-0754 J9 ASTRON ASTROPHYS REV JI Astron. Astrophys. Rev. PD JUN PY 2009 VL 17 IS 2 BP 105 EP 147 DI 10.1007/s00159-009-0018-0 PG 43 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 454EW UT WOS:000266666200001 ER PT J AU Marti-Vidal, I Marcaide, JM Alberdi, A Guirado, JC Perez-Torres, MA Ros, E Shapiro, II Beswick, RJ Muxlow, TWB Pedlar, A Argo, MK Immler, S Panagia, N Stockdale, CJ Sramek, RA Van Dyk, S Weiler, KW AF Marti-Vidal, I. Marcaide, J. M. Alberdi, A. Guirado, J. C. Perez-Torres, M. A. Ros, E. Shapiro, I. I. Beswick, R. J. Muxlow, T. W. B. Pedlar, A. Argo, M. K. Immler, S. Panagia, N. Stockdale, C. J. Sramek, R. A. Van Dyk, S. Weiler, K. W. TI 23 GHz VLBI observations of SN 2008ax (Research Note) SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE galaxies: individual: NGC 4490; radio continuum: stars; supernovae: individual: SN 2008ax; supernovae: general AB We report on phase-referenced 23 GHz Very-Long-Baseline-Interferometry (VLBI) observations of the type IIb supernova SN 2008ax, made with the Very Long Baseline Array (VLBA) on 2 April 2008 (33 days after explosion). These observations resulted in a marginal detection of the supernova. The total flux density recovered from our VLBI image is 0.8 +/- 0.3 mJy (one standard deviation). As it appears, the structure may be interpreted as either a core-jet or a double source. However, the supernova structure could be somewhat confused with a possible close by noise peak. In such a case, the recovered flux density would decrease to 0.48 +/- 0.12 mJy, compatible with the flux densities measured with the VLA at epochs close in time to our VLBI observations. The lowest average expansion velocities derived from our observations are (1.90 +/- 0.30) x 10(5) km s(-1) (case of a double source) and (5.2 +/- 1.3) x 10(4) km s(-1) (taking the weaker source component as a spurious, close by, noise peak, which is the more likely interpretation). These velocities are 7.3 and 2 times higher, respectively, than the maximum ejecta velocity inferred from optical-line observations. C1 [Marti-Vidal, I.; Marcaide, J. M.; Guirado, J. C.; Ros, E.] Univ Valencia, Dpt Astron & Astrofis, E-46100 Burjassot, Spain. [Weiler, K. W.] USN, Res Lab, Washington, DC 20375 USA. [Van Dyk, S.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Shapiro, I. I.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Marti-Vidal, I.; Ros, E.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Panagia, N.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Beswick, R. J.; Muxlow, T. W. B.; Pedlar, A.] Jodrell Bank Observ, Macclesfield SK11 9DL, Cheshire, England. [Alberdi, A.; Perez-Torres, M. A.] CSIC, Inst Astrofis Andalucia, E-18008 Granada, Spain. [Sramek, R. A.] Natl Radio Astron Observ, Socorro, NM 87801 USA. [Stockdale, C. J.] Marquette Univ, Dept Phys, Milwaukee, WI 53201 USA. [Immler, S.] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA. [Argo, M. K.] Curtin Univ Technol, Dept Imaging & Appl Phys, Bentley, WA 6845, Australia. [Panagia, N.] INAF Osservatorio Astrofis Catania, I-95123 Catania, Italy. RP Marti-Vidal, I (reprint author), Univ Valencia, Dpt Astron & Astrofis, C Dr Moliner 50, E-46100 Burjassot, Spain. EM I.Marti-Vidal@uv.es RI Marti-Vidal, Ivan/A-8799-2017; OI Marti-Vidal, Ivan/0000-0003-3708-9611; Muxlow, Thomas/0000-0001-5797-8796; Ros, Eduardo/0000-0001-9503-4892; Argo, Megan/0000-0003-3594-0214; Van Dyk, Schuyler/0000-0001-9038-9950 FU Spanish DGICYT [AYA2006-14986-CO2-01, AYA2006-14986-C02-02]; Office of Naval Research; Alexander von Humboldt Foundation FX The National Radio Astronomy Observatory is a facility of the National Science Foundation, operated under cooperative agreement by Associated Universities, Inc. This work has been partially funded by grants AYA2006-14986-CO2-01 and AYA2006-14986-C02-02 of the Spanish DGICYT. K. W. W. thanks the Office of Naval Research for the 6.1 funding supporting this research. I. M. V. is a fellow of the Alexander von Humboldt Foundation. NR 15 TC 5 Z9 5 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 JUN PY 2009 VL 499 IS 3 BP 649 EP 652 DI 10.1051/0004-6361/200912034 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 455BK UT WOS:000266730600006 ER PT J AU Cuypers, J Aerts, C De Cat, P De Ridder, J Goossens, K Schoenaers, C Uytterhoeven, K Acke, B Davignon, G Debosscher, J Decin, L De Meester, W Deroo, P Drummond, R Kolenberg, K Lefever, K Raskin, G Reyniers, M Saesen, S Vandenbussche, B Van Malderen, R Verhoelst, T Van Winckel, H Waelkens, C AF Cuypers, J. Aerts, C. De Cat, P. De Ridder, J. Goossens, K. Schoenaers, C. Uytterhoeven, K. Acke, B. Davignon, G. Debosscher, J. Decin, L. De Meester, W. Deroo, P. Drummond, R. Kolenberg, K. Lefever, K. Raskin, G. Reyniers, M. Saesen, S. Vandenbussche, B. Van Malderen, R. Verhoelst, T. Van Winckel, H. Waelkens, C. TI Long-term photometric monitoring with the Mercator telescope Frequencies and multicolour amplitudes of gamma Doradus stars SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE stars: variables: general; stars: oscillations; stars: individual: gamma Doradus; techniques: photometric ID TIME-SERIES ANALYSIS; MULTISITE CAMPAIGN; SPACED DATA; VARIABLES; SPECTROSCOPY; PULSATIONS; CANDIDATES; OSCILLATIONS; CALIBRATION AB Context. gamma Dor stars are excellent targets for asteroseismology since the gravity modes present in these stars probe the deep stellar interiors. Mode identification will improve the knowledge of these stars considerably. Aims. A selected group of gamma Dor stars and some candidates were observed with the Mercator telescope to find and/or confirm the periodicities in the light variations and to derive reliable amplitude ratios in different pass bands. Methods. A frequency analysis was performed on all new data obtained in the Geneva photometric system. In order to have more reliable and accurate frequencies, the new data were combined with similar data from the literature and with Hipparcos observations. A set of frequencies that minimized the residuals in a harmonic fit was searched for while allowing means and amplitudes to vary from one observation set to another. Results. Frequencies and amplitudes in the photometric passbands of the Geneva system are given for 21 gamma Dor stars. We report the discovery of HD 74504 as a newly found gamma Dor star. Conclusions. Our study provides the first extensive multicolour database for the understanding of gravity modes in F-type stars. C1 [Cuypers, J.; De Cat, P.; Schoenaers, C.] Koninklijke Sterrenwacht Belgie, B-1180 Brussels, Belgium. [Aerts, C.; De Ridder, J.; Goossens, K.; Uytterhoeven, K.; Acke, B.; Davignon, G.; Debosscher, J.; Decin, L.; De Meester, W.; Deroo, P.; Drummond, R.; Kolenberg, K.; Lefever, K.; Raskin, G.; Reyniers, M.; Saesen, S.; Vandenbussche, B.; Van Malderen, R.; Verhoelst, T.; Van Winckel, H.; Waelkens, C.] Katholieke Univ Leuven, Sterrekundig Inst, B-3001 Heverlee, Belgium. [Aerts, C.] Radboud Univ Nijmegen, Dept Astrophys, NL-6500 GL Nijmegen, Netherlands. [Schoenaers, C.] Univ Oxford, Oxford OX1 3RH, England. [Uytterhoeven, K.; Davignon, G.; Raskin, G.] MERCATOR Telescope, Santa Cruz De La Palma 38700, Spain. [Reyniers, M.; Van Malderen, R.] Koninklijk Meteorol Inst, B-1180 Brussels, Belgium. [Kolenberg, K.] Univ Vienna, Inst Astron, A-1180 Vienna, Austria. [Drummond, R.; Lefever, K.] Belgisch Inst Ruimte Aeron, B-1180 Brussels, Belgium. [Uytterhoeven, K.] IRFU DSM CEA Saclay, Serv Astrophys, F-91191 Gif Sur Yvette, France. [Deroo, P.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Cuypers, J (reprint author), Koninklijke Sterrenwacht Belgie, Ringlaan 3, B-1180 Brussels, Belgium. EM Jan.Cuypers@oma.be RI Van Winckel, Hans/I-7863-2013 OI Van Winckel, Hans/0000-0001-5158-9327 FU Fund for Scientific Research-Flanders (FWO) [G.0178.02, G.0332.06]; Research Council of K.U. Leuven [GOA/2008/04]; European Research Council [FP7/2007-2013, 227224] FX This research was made possible thanks to the financial support from the Fund for Scientific Research-Flanders (FWO), under projects G.0178.02 and G.0332.06. The Leuven authors additionally are supported by the Research Council of K.U. Leuven under grant GOA/2008/04. The research leading to these results has received funding from the European Research Council under the European Community's Seventh Framework Programme (FP7/2007-2013)/ERC grant agreement No. 227224 (PROSPERITY). We are indebted to our colleagues of the Geneva Observatory who reduced the mercator data. This research has made use of the NASA's Astrophysics Data System and the SIMBAD astronomical database operated at the CDS in Strasbourg, France. NR 41 TC 19 Z9 19 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 JUN PY 2009 VL 499 IS 3 BP 967 EP 982 DI 10.1051/0004-6361/200911691 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 455BK UT WOS:000266730600037 ER PT J AU Agol, E Gogarten, SM Gorjian, V Kimball, A AF Agol, Eric Gogarten, Stephanie M. Gorjian, Varoujan Kimball, Amy TI SPITZER OBSERVATIONS OF A GRAVITATIONALLY LENSED QUASAR, QSO 2237+0305 SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; galaxies: active; gravitational lensing; infrared: general; quasars: individual (QSO 2237+0305); radiation mechanisms: thermal ID ACTIVE GALACTIC NUCLEI; ACCRETION DISKS; ENERGY-DISTRIBUTIONS; SPACE-TELESCOPE; MICROLENSING VARIABILITY; INFRARED SPECTROGRAPH; LENSING EXPERIMENT; EINSTEIN CROSS; EQUIVALENT-TO; EMISSION AB The four-image gravitationally lensed quasar QSO 2237+0305 is microlensed by stars in the lens galaxy. The amplitude of microlensing variability can be used to infer the relative size of the quasar as a function of wavelength; this provides a test of quasar models. Toward this end, we present Spitzer Space Telescope Infrared Spectrograph and Infrared Array Camera (IRAC) observations of QSO 2237+0305, finding the following. (1) The infrared (IR) spectral energy distribution (SED) is similar to that of other bright radio-quiet quasars, contrary to an earlier claim. (2) A dusty torus model with a small opening angle fits the overall shape of the IR SED well, but the quantitative agreement is poor due to an offset in wavelength of the silicate feature. (3) The flux ratios of the four lensed images can be derived from the IRAC data despite being unresolved. We find that the near-IR fluxes are increasingly affected by microlensing toward shorter wavelengths. (4) The wavelength dependence of the IRAC flux ratios is consistent with the standard quasar model in which an accretion disk and a dusty torus both contribute near 1 mu m in the rest frame. This is also consistent with recent IR spectropolarimetry of nearby quasars. C1 [Agol, Eric; Gogarten, Stephanie M.; Kimball, Amy] Univ Washington, Dept Astron, Seattle, WA 98195 USA. [Gorjian, Varoujan] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Agol, E (reprint author), Univ Washington, Dept Astron, Box 351580, Seattle, WA 98195 USA. EM agol@astro.washington.edu RI Agol, Eric/B-8775-2013; OI Agol, Eric/0000-0002-0802-9145; Gogarten, Stephanie/0000-0002-7231-9745 FU NASA FX This work is based in part on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology under a contract with NASA. Support for this work was provided by NASA through an award issued by JPL/Caltech. E. A. acknowledges the hospitality of the Institute for Theory and Computation at the Harvard-Smithsonian Center for Astrophysics where a portion of this work was completed. The authors thank Ski Antonucci, Zeljko Ivezic, Chris Kochanek, and Julian Krolik, for helpful discussions. We thank Chris Kochanek for providing a deconvolved H-band image from the CASTLES database and Jacopo Fritz for providing the grid of dusty torus models from his paper. We thank the OGLE collaboration for making their data on Q2237+0305 available on their web site. We thank Joachim Wambsganss for sharing his code for simulating microlensing by random star fields and a helpful referee report. We thank Alex Eigenbrod for sharing the wavelength-dependent flux ratios measured with VLT. We thank Cathy Trott for sharing her model prediction for the flux ratios prior to publication. We thank Bruce Draine for making his ISM dust opacity model available on his web site. NR 51 TC 27 Z9 27 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUN 1 PY 2009 VL 697 IS 2 BP 1010 EP 1019 DI 10.1088/0004-637X/697/2/1010 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 446YT UT WOS:000266159500006 ER PT J AU Atwood, WB Abdo, AA Ackermann, M Althouse, W Anderson, B Axelsson, M Baldini, L Ballet, J Band, DL Barbiellini, G Bartelt, J Bastieri, D Baughman, BM Bechtol, K Bederede, D Bellardi, F Bellazzini, R Berenji, B Bignami, GF Bisello, D Bissaldi, E Blandford, RD Bloom, ED Bogart, JR Bonamente, E Bonnell, J Borgland, AW Bouvier, A Bregeon, J Brez, A Brigida, M Bruel, P Burnett, TH Busetto, G Caliandro, GA Cameron, RA Caraveo, PA Carius, S Carlson, P Casandjian, JM Cavazzuti, E Ceccanti, M Cecchi, C Charles, E Chekhtman, A Cheung, CC Chiang, J Chipaux, R Cillis, AN Ciprini, S Claus, R Cohen-Tanugi, J Condamoor, S Conrad, J Corbet, R Corucci, L Costamante, L Cutini, S Davis, DS Decotigny, D DeKlotz, M Dermer, CD De Angelis, A Digel, SW Silva, EDCE Drell, PS Dubois, R Dumora, D Edmonds, Y Fabiani, D Farnier, C Favuzzi, C Flath, DL Fleury, P Focke, WB Funk, S Fusco, P Gargano, F Gasparrini, D Gehrels, N Gentit, FX Germani, S Giebels, B Giglietto, N Giommi, P Giordano, F Glanzman, T Godfrey, G Grenier, IA Grondin, MH Grove, JE Guillemot, L Guiriec, S Haller, G Harding, AK Hart, PA Hays, E Healey, SE Hirayama, M Hjalmarsdotter, L Horn, R Hughes, RE Johannesson, G Johansson, G Johnson, AS Johnson, RP Johnson, TJ Johnson, WN Kamae, T Katagiri, H Kataoka, J Kavelaars, A Kawai, N Kelly, H Kerr, M Klamra, W Knodlseder, J Kocian, ML Komin, N Kuehn, F Kuss, M Landriu, D Latronico, L Lee, B Lee, SH Lemoine-Goumard, M Lionetto, AM Longo, F Loparco, F Lott, B Lovellette, MN Lubrano, P Madejski, GM Makeev, A Marangelli, B Massai, MM Mazziotta, MN McEnery, JE Menon, N Meurer, C Michelson, PF Minuti, M Mirizzi, N Mitthumsiri, W Mizuno, T Moiseev, AA Monte, C Monzani, ME Moretti, E Morselli, A Moskalenko, IV Murgia, S Nakamori, T Nishino, S Nolan, PL Norris, JP Nuss, E Ohno, M Ohsugi, T Omodei, N Orlando, E Ormes, JF Paccagnella, A Paneque, D Panetta, JH Parent, D Pearce, M Pepe, M Perazzo, A Pesce-Rollins, M Picozza, P Pieri, L Pinchera, M Piron, F Porter, TA Poupard, L Raino, S Rando, R Rapposelli, E Razzano, M Reimer, A Reimer, O Reposeur, T Reyes, LC Ritz, S Rochester, LS Rodriguez, AY Romani, RW Roth, M Russell, JJ Ryde, F Sabatini, S Sadrozinski, HFW Sanchez, D Sander, A Sapozhnikov, L Parkinson, PMS Scargle, JD Schalk, TL Scolieri, G Sgro, C Share, GH Shaw, M Shimokawabe, T Shrader, C Sierpowska-Bartosik, A Siskind, EJ Smith, DA Smith, PD Spandre, G Spinelli, P Starck, JL Stephens, TE Strickman, MS Strong, AW Suson, DJ Tajima, H Takahashi, H Takahashi, T Tanaka, T Tenze, A Tether, S Thayer, JB Thayer, JG Thompson, DJ Tibaldo, L Tibolla, O Torres, DF Tosti, G Tramacere, A Turri, M Usher, TL Vilchez, N Vitale, V Wang, P Watters, K Winer, BL Wood, KS Ylinen, T Ziegler, M AF Atwood, W. B. Abdo, A. A. Ackermann, M. Althouse, W. Anderson, B. Axelsson, M. Baldini, L. Ballet, J. Band, D. L. Barbiellini, G. Bartelt, J. Bastieri, D. Baughman, B. M. Bechtol, K. Bederede, D. Bellardi, F. Bellazzini, R. Berenji, B. Bignami, G. F. Bisello, D. Bissaldi, E. Blandford, R. D. Bloom, E. D. Bogart, J. R. Bonamente, E. Bonnell, J. Borgland, A. W. Bouvier, A. Bregeon, J. Brez, A. Brigida, M. Bruel, P. Burnett, T. H. Busetto, G. Caliandro, G. A. Cameron, R. A. Caraveo, P. A. Carius, S. Carlson, P. Casandjian, J. M. Cavazzuti, E. Ceccanti, M. Cecchi, C. Charles, E. Chekhtman, A. Cheung, C. C. Chiang, J. Chipaux, R. Cillis, A. N. Ciprini, S. Claus, R. Cohen-Tanugi, J. Condamoor, S. Conrad, J. Corbet, R. Corucci, L. Costamante, L. Cutini, S. Davis, D. S. Decotigny, D. DeKlotz, M. Dermer, C. D. De Angelis, A. Digel, S. W. Silva, E. Do Couto E. Drell, P. S. Dubois, R. Dumora, D. Edmonds, Y. Fabiani, D. Farnier, C. Favuzzi, C. Flath, D. L. Fleury, P. Focke, W. B. Funk, S. Fusco, P. Gargano, F. Gasparrini, D. Gehrels, N. Gentit, F. -X. Germani, S. Giebels, B. Giglietto, N. Giommi, P. Giordano, F. Glanzman, T. Godfrey, G. Grenier, I. A. Grondin, M. -H. Grove, J. E. Guillemot, L. Guiriec, S. Haller, G. Harding, A. K. Hart, P. A. Hays, E. Healey, S. E. Hirayama, M. Hjalmarsdotter, L. Horn, R. Hughes, R. E. Johannesson, G. Johansson, G. Johnson, A. S. Johnson, R. P. Johnson, T. J. Johnson, W. N. Kamae, T. Katagiri, H. Kataoka, J. Kavelaars, A. Kawai, N. Kelly, H. Kerr, M. Klamra, W. Knoedlseder, J. Kocian, M. L. Komin, N. Kuehn, F. Kuss, M. Landriu, D. Latronico, L. Lee, B. Lee, S. -H. Lemoine-Goumard, M. Lionetto, A. M. Longo, F. Loparco, F. Lott, B. Lovellette, M. N. Lubrano, P. Madejski, G. M. Makeev, A. Marangelli, B. Massai, M. M. Mazziotta, M. N. McEnery, J. E. Menon, N. Meurer, C. Michelson, P. F. Minuti, M. Mirizzi, N. Mitthumsiri, W. Mizuno, T. Moiseev, A. A. Monte, C. Monzani, M. E. Moretti, E. Morselli, A. Moskalenko, I. V. Murgia, S. Nakamori, T. Nishino, S. Nolan, P. L. Norris, J. P. Nuss, E. Ohno, M. Ohsugi, T. Omodei, N. Orlando, E. Ormes, J. F. Paccagnella, A. Paneque, D. Panetta, J. H. Parent, D. Pearce, M. Pepe, M. Perazzo, A. Pesce-Rollins, M. Picozza, P. Pieri, L. Pinchera, M. Piron, F. Porter, T. A. Poupard, L. Raino, S. Rando, R. Rapposelli, E. Razzano, M. Reimer, A. Reimer, O. Reposeur, T. Reyes, L. C. Ritz, S. Rochester, L. S. Rodriguez, A. Y. Romani, R. W. Roth, M. Russell, J. J. Ryde, F. Sabatini, S. Sadrozinski, H. F. -W. Sanchez, D. Sander, A. Sapozhnikov, L. Parkinson, P. M. Saz Scargle, J. D. Schalk, T. L. Scolieri, G. Sgro, C. Share, G. H. Shaw, M. Shimokawabe, T. Shrader, C. Sierpowska-Bartosik, A. Siskind, E. J. Smith, D. A. Smith, P. D. Spandre, G. Spinelli, P. Starck, J. -L. Stephens, T. E. Strickman, M. S. Strong, A. W. Suson, D. J. Tajima, H. Takahashi, H. Takahashi, T. Tanaka, T. Tenze, A. Tether, S. Thayer, J. B. Thayer, J. G. Thompson, D. J. Tibaldo, L. Tibolla, O. Torres, D. F. Tosti, G. Tramacere, A. Turri, M. Usher, T. L. Vilchez, N. Vitale, V. Wang, P. Watters, K. Winer, B. L. Wood, K. S. Ylinen, T. Ziegler, M. TI THE LARGE AREA TELESCOPE ON THE FERMI GAMMA-RAY SPACE TELESCOPE MISSION SO ASTROPHYSICAL JOURNAL LA English DT Review DE cosmic rays; galaxies: active; Galaxy: general; gamma rays: observations; Sun: X-rays, gamma rays; telescopes ID EXTRAGALACTIC BACKGROUND LIGHT; VERY-HIGH-ENERGY; TIME-DIFFERENCING TECHNIQUE; INVERSE COMPTON-SCATTERING; FLIGHT ENGINEERING MODEL; PROBING GALAXY FORMATION; PRIMORDIAL BLACK-HOLES; DARK-MATTER; EGRET DATA; X-RAY AB The Large Area Telescope (Fermi/LAT, hereafter LAT), the primary instrument on the Fermi Gamma-ray Space Telescope (Fermi) mission, is an imaging, wide field-of-view (FoV), high-energy gamma-ray telescope, covering the energy range from below 20 MeV to more than 300 GeV. The LAT was built by an international collaboration with contributions from space agencies, high-energy particle physics institutes, and universities in France, Italy, Japan, Sweden, and the United States. This paper describes the LAT, its preflight expected performance, and summarizes the key science objectives that will be addressed. On-orbit performance will be presented in detail in a subsequent paper. The LAT is a pair-conversion telescope with a precision tracker and calorimeter, each consisting of a 4 x 4 array of 16 modules, a segmented anticoincidence detector that covers the tracker array, and a programmable trigger and data acquisition system. Each tracker module has a vertical stack of 18 (x, y) tracking planes, including two layers (x and y) of single-sided silicon strip detectors and high-Z converter material (tungsten) per tray. Every calorimeter module has 96 CsI(Tl) crystals, arranged in an eight-layer hodoscopic configuration with a total depth of 8.6 radiation lengths, giving both longitudinal and transverse information about the energy deposition pattern. The calorimeter's depth and segmentation enable the high-energy reach of the LAT and contribute significantly to background rejection. The aspect ratio of the tracker (height/width) is 0.4, allowing a large FoV (2.4 sr) and ensuring that most pair-conversion showers initiated in the tracker will pass into the calorimeter for energy measurement. Data obtained with the LAT are intended to (1) permit rapid notification of high-energy gamma-ray bursts and transients and facilitate monitoring of variable sources, (2) yield an extensive catalog of several thousand high-energy sources obtained from an all-sky survey, (3) measure spectra from 20 MeV to more than 50 GeV for several hundred sources, (4) localize point sources to 0.3-2 arcmin, (5) map and obtain spectra of extended sources such as SNRs, molecular clouds, and nearby galaxies, (6) measure the diffuse isotropic gamma-ray background up to TeV energies, and (7) explore the discovery space for dark matter. C1 [Atwood, W. B.; Anderson, B.; Johnson, R. P.; Porter, T. A.; Sadrozinski, H. F. -W.; Parkinson, P. M. Saz; Schalk, T. L.; Ziegler, M.] Univ Calif Santa Cruz, Santa Cruz Inst Particle Phys, Dept Phys, Santa Cruz, CA 95064 USA. [Atwood, W. B.; Anderson, B.; Johnson, R. P.; Porter, T. A.; Sadrozinski, H. F. -W.; Parkinson, P. M. Saz; Schalk, T. L.; Ziegler, M.] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA. [Abdo, A. A.; Chekhtman, A.; Dermer, C. D.; Grove, J. E.; Johnson, W. N.; Makeev, A.; Share, G. H.; Strickman, M. S.; Wood, K. S.] USN, Res Lab, Div Space Sci, Washington, DC 20375 USA. [Ackermann, M.; Althouse, W.; Bartelt, J.; Bechtol, K.; Berenji, B.; Blandford, R. D.; Bloom, E. D.; Bogart, J. R.; Borgland, A. W.; Bouvier, A.; Cameron, R. A.; Charles, E.; Chiang, J.; Claus, R.; Condamoor, S.; Costamante, L.; Digel, S. W.; Silva, E. Do Couto E.; Drell, P. S.; Dubois, R.; Edmonds, Y.; Flath, D. L.; Focke, W. B.; Funk, S.; Glanzman, T.; Godfrey, G.; Haller, G.; Hart, P. A.; Healey, S. E.; Johannesson, G.; Johnson, A. S.; Kamae, T.; Kavelaars, A.; Kelly, H.; Kocian, M. L.; Lee, S. -H.; Madejski, G. M.; Michelson, P. F.; Mitthumsiri, W.; Monzani, M. E.; Moskalenko, I. V.; Murgia, S.; Nolan, P. L.; Panetta, J. H.; Perazzo, A.; Reimer, A.; Reimer, O.; Rochester, L. S.; Romani, R. W.; Russell, J. J.; Sapozhnikov, L.; Shaw, M.; Tajima, H.; Tanaka, T.; Tether, S.; Thayer, J. B.; Thayer, J. G.; Tramacere, A.; Turri, M.; Usher, T. L.; Wang, P.; Watters, K.] Stanford Univ, WW Hansen Expt Phys Lab, Kavli Inst Particle Astrophys & Cosmol, Dept Phys, Stanford, CA 94305 USA. [Ackermann, M.; Althouse, W.; Bartelt, J.; Bechtol, K.; Berenji, B.; Blandford, R. D.; Bloom, E. D.; Bogart, J. R.; Borgland, A. W.; Bouvier, A.; Cameron, R. A.; Charles, E.; Chiang, J.; Claus, R.; Condamoor, S.; Costamante, L.; Digel, S. W.; Silva, E. Do Couto E.; Drell, P. S.; Dubois, R.; Edmonds, Y.; Flath, D. L.; Focke, W. B.; Funk, S.; Glanzman, T.; Godfrey, G.; Haller, G.; Hart, P. A.; Healey, S. E.; Johannesson, G.; Johnson, A. S.; Kamae, T.; Kavelaars, A.; Kelly, H.; Kocian, M. L.; Lee, S. -H.; Madejski, G. M.; Michelson, P. F.; Mitthumsiri, W.; Monzani, M. E.; Moskalenko, I. V.; Murgia, S.; Nolan, P. L.; Panetta, J. H.; Perazzo, A.; Reimer, A.; Reimer, O.; Rochester, L. S.; Romani, R. W.; Russell, J. J.; Sapozhnikov, L.; Shaw, M.; Tajima, H.; Tanaka, T.; Tether, S.; Thayer, J. B.; Thayer, J. G.; Tramacere, A.; Turri, M.; Usher, T. L.; Wang, P.; Watters, K.] Stanford Univ, SLAC Natl Accelerator Lab, Stanford, CA 94305 USA. [Axelsson, M.; Hjalmarsdotter, L.] Stockholm Observ, SE-10691 Stockholm, Sweden. [Baldini, L.; Bellardi, F.; Bellazzini, R.; Bregeon, J.; Brez, A.; Ceccanti, M.; Corucci, L.; Fabiani, D.; Kuss, M.; Latronico, L.; Massai, M. M.; Menon, N.; Minuti, M.; Omodei, N.; Pesce-Rollins, M.; Pinchera, M.; Rapposelli, E.; Razzano, M.; Sgro, C.; Spandre, G.; Tenze, A.] Ist Nazl Fis Nucl, Sez Pisa, I-56127 Pisa, Italy. [Ballet, J.; Casandjian, J. M.; Grenier, I. A.; Komin, N.; Landriu, D.; Poupard, L.; Starck, J. -L.] Univ Paris Diderot, Lab AIM, CEA IRFU CNRS, Serv Astrophys,CEA Saclay, F-91191 Gif Sur Yvette, France. [Band, D. L.; Moiseev, A. A.; Shrader, C.] NASA, Goddard Space Flight Ctr, CRESST, Greenbelt, MD 20771 USA. [Barbiellini, G.; Longo, F.; Moretti, E.] Ist Nazl Fis Nucl, Sez Trieste, I-34127 Trieste, Italy. [Barbiellini, G.; Longo, F.; Moretti, E.] Univ Trieste, Dipartmento Fis, I-34127 Trieste, Italy. [Bastieri, D.; Bisello, D.; Busetto, G.; Paccagnella, A.; Pieri, L.; Rando, R.; Tibaldo, L.] Ist Nazl Fis Nucl, Sez Padova, I-35131 Padua, Italy. [Bastieri, D.; Bisello, D.; Busetto, G.; Rando, R.; Tibaldo, L.] Univ Padua, Dipartimento Fis G Galilei, I-35131 Padua, Italy. [Baughman, B. M.; Hughes, R. E.; Kuehn, F.; Sander, A.; Smith, P. D.; Winer, B. L.] Ohio State Univ, Dept Phys, Ctr Cosmol & Astroparticle Phys, Columbus, OH 43210 USA. [Bederede, D.] CEA Saclay, IRFU Dir, F-91191 Gif Sur Yvette, France. [Bignami, G. F.] IUSS, I-27100 Pavia, Italy. [Bissaldi, E.; Orlando, E.; Strong, A. W.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Bonamente, E.; Cecchi, C.; Ciprini, S.; Germani, S.; Lubrano, P.; Pepe, M.; Tosti, G.] Ist Nazl Fis Nucl, Sez Perugia, I-60123 Perugia, Italy. [Bonamente, E.; Cecchi, C.; Ciprini, S.; Germani, S.; Lubrano, P.; Pepe, M.; Tosti, G.] Univ Perugia, Dipartimento Fis, I-06123 Perugia, Italy. [Brigida, M.; Caliandro, G. A.; Favuzzi, C.; Fusco, P.; Giglietto, N.; Giordano, F.; Loparco, F.; Marangelli, B.; Mirizzi, N.; Monte, C.; Raino, S.; Spinelli, P.] Univ Politecn Bari, Dipartimento Fis M Merlin, I-70126 Bari, Italy. [Brigida, M.; Caliandro, G. A.; Favuzzi, C.; Fusco, P.; Gargano, F.; Giglietto, N.; Giordano, F.; Loparco, F.; Lovellette, M. N.; Marangelli, B.; Mazziotta, M. N.; Mirizzi, N.; Monte, C.; Raino, S.; Spinelli, P.] Ist Nazl Fis Nucl, Sez Bari, I-70126 Bari, Italy. [Bruel, P.; Decotigny, D.; Fleury, P.; Giebels, B.; Sanchez, D.] Ecole Polytech, CNRS, Lab Leprince Ringuet, IN2P3, F-91128 Palaiseau, France. [Burnett, T. H.; Kerr, M.; Roth, M.] Univ Washington, Dept Phys, Seattle, WA 98195 USA. [Caraveo, P. A.] Ist Astrofis Spaziale & Fis Cosm, INAF, I-20133 Milan, Italy. [Carius, S.; Johansson, G.; Ylinen, T.] Univ Kalmar, Sch Pure & Appl Nat Sci, SE-39182 Kalmar, Sweden. [Carlson, P.; Conrad, J.; Klamra, W.; Pearce, M.; Ryde, F.; Ylinen, T.] Royal Inst Technol, KTH, Dept Phys, SE-10691 Stockholm, Sweden. [Cavazzuti, E.; Cutini, S.; Gasparrini, D.; Giommi, P.] Sci Data Ctr, ASI, I-00044 Frascati, Italy. [Chekhtman, A.; Makeev, A.] George Mason Univ, Fairfax, VA 22030 USA. [Chipaux, R.; Cohen-Tanugi, J.; Farnier, C.; Guiriec, S.; Komin, N.; Nuss, E.; Piron, F.] CEA Saclay, IRFU SEDI, F-91191 Gif Sur Yvette, France. [Cohen-Tanugi, J.; Farnier, C.; Guiriec, S.; Komin, N.; Nuss, E.; Piron, F.] Univ Montpellier 2, Lab Phys Theor & Astroparticules, CNRS, IN2P3, Montpellier, France. [Conrad, J.; Meurer, C.] Stockholm Univ, Dept Phys, SE-10691 Stockholm, Sweden. [Hirayama, M.] Univ Maryland, Ctr Space Sci & Technol, Baltimore, MD 21250 USA. [DeKlotz, M.; Horn, R.; Menon, N.] Stellar Solut Inc, Palo Alto, CA 94306 USA. [De Angelis, A.] Univ Udine, Dipartimento Fis, I-33100 Udine, Italy. [De Angelis, A.] Ist Nazl Fis Nucl, Sez Trieste, Grp Collegato Udine, I-33100 Udine, Italy. [Dumora, D.; Grondin, M. -H.; Guillemot, L.; Lemoine-Goumard, M.; Lott, B.; Parent, D.; Reposeur, T.; Smith, D. A.] CEN Bordeaux Gradignan, CNRS IN2P3, UMR 5797, F-33175 Gradignan, France. [Dumora, D.; Grondin, M. -H.; Guillemot, L.; Lemoine-Goumard, M.; Lott, B.; Parent, D.; Reposeur, T.; Smith, D. A.] Univ Bordeaux, Ctr Etud Nucl Bordeaux Gradignan, UMR 5797, F-33175 Gradignan, France. [Johnson, T. J.; Ritz, S.] Univ Maryland, College Pk, MD 20742 USA. [Gentit, F. -X.] CEA Saclay, IRFU, Serv Phys Particules, F-91191 Gif Sur Yvette, France. [Katagiri, H.; Mizuno, T.; Nishino, S.; Ohsugi, T.; Takahashi, H.] Hiroshima Univ, Dept Phys Sci, Higashihiroshima 7398526, Japan. [Katagiri, H.; Mizuno, T.; Nishino, S.; Ohsugi, T.; Takahashi, H.] Hiroshima Univ, Hiroshima Astrophys Sci Ctr, Higashihiroshima 7398526, Japan. [Kataoka, J.; Kawai, N.; Nakamori, T.; Shimokawabe, T.] Tokyo Inst Technol, Dept Phys, Tokyo 1528551, Japan. [Kawai, N.] RIKEN, Inst Phys & Chem Res, Cosm Radiat Lab, Saitama 3510198, Japan. [Knoedlseder, J.; Vilchez, N.] CNRS UPS, Ctr Etud Spatiale Rayonnements, F-31028 Toulouse 4, France. [Lee, B.] Orbital Network Engn, Cupertino, CA 95014 USA. [Lionetto, A. M.; Morselli, A.; Picozza, P.; Sabatini, S.; Vitale, V.] Ist Nazl Fis Nucl, Sez Roma Tor Vergata, I-00133 Rome, Italy. [Lionetto, A. M.; Morselli, A.; Picozza, P.; Sabatini, S.; Vitale, V.] Univ Roma Tor Vergata, Dipartimento Fis, I-00133 Rome, Italy. [Norris, J. P.; Ormes, J. F.] Univ Denver, Dept Phys & Astron, Denver, CO 80208 USA. [Ohno, M.; Takahashi, T.] Inst Space & Astronaut Sci, JAXA, Sagamihara, Kanagawa 2298510, Japan. [Paccagnella, A.] Univ Padua, Dipartimento Ingn Informaz, I-35131 Padua, Italy. [Reyes, L. C.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA. [Rodriguez, A. Y.; Sierpowska-Bartosik, A.; Torres, D. F.] Inst Ciencies Espai, IEEC CSIC, Barcelona 08193, Spain. [Scargle, J. D.] NASA, Ames Res Ctr, Div Space Sci, Moffett Field, CA 94035 USA. [Scolieri, G.] Ist Nazl Fis Nucl, I-06123 Perugia, Italy. [Share, G. H.] Praxis Inc, Alexandria, VA 22303 USA. [Siskind, E. J.] NYCB Real Time Comp Inc, Lattingtown, NY 11560 USA. [Suson, D. J.] Purdue Univ Calumet, Dept Chem & Phys, Hammond, IN 46323 USA. [Tibolla, O.] Heidelberg Univ, D-69117 Heidelberg, Germany. [Torres, D. F.] ICREA, Barcelona, Spain. [Tramacere, A.] CIFS, I-10133 Turin, Italy. RP Michelson, PF (reprint author), Univ Calif Santa Cruz, Santa Cruz Inst Particle Phys, Dept Phys, Santa Cruz, CA 95064 USA. EM peterm@stanford.edu RI Komin, Nukri/J-6781-2015; Hays, Elizabeth/D-3257-2012; Johnson, Neil/G-3309-2014; Reimer, Olaf/A-3117-2013; Funk, Stefan/B-7629-2015; Gargano, Fabio/O-8934-2015; Johannesson, Gudlaugur/O-8741-2015; Loparco, Francesco/O-8847-2015; Moskalenko, Igor/A-1301-2007; Mazziotta, Mario /O-8867-2015; Sgro, Carmelo/K-3395-2016; Bissaldi, Elisabetta/K-7911-2016; Torres, Diego/O-9422-2016; Nolan, Patrick/A-5582-2009; Kuss, Michael/H-8959-2012; giglietto, nicola/I-8951-2012; Tosti, Gino/E-9976-2013; Rando, Riccardo/M-7179-2013; Starck, Jean-Luc/D-9467-2011; Thompson, David/D-2939-2012; Harding, Alice/D-3160-2012; Gehrels, Neil/D-2971-2012; McEnery, Julie/D-6612-2012; Chipaux, Remi/G-1145-2010; Baldini, Luca/E-5396-2012; lubrano, pasquale/F-7269-2012; Morselli, Aldo/G-6769-2011 OI Berenji, Bijan/0000-0002-4551-772X; Gasparrini, Dario/0000-0002-5064-9495; Tramacere, Andrea/0000-0002-8186-3793; Baldini, Luca/0000-0002-9785-7726; Pesce-Rollins, Melissa/0000-0003-1790-8018; Axelsson, Magnus/0000-0003-4378-8785; Moretti, Elena/0000-0001-5477-9097; Cutini, Sara/0000-0002-1271-2924; Sgro', Carmelo/0000-0001-5676-6214; Bignami, Giovanni/0000-0001-9582-2450; Picozza, Piergiorgio/0000-0002-7986-3321; Stephens, Thomas/0000-0003-3065-6871; SPINELLI, Paolo/0000-0001-6688-8864; giommi, paolo/0000-0002-2265-5003; De Angelis, Alessandro/0000-0002-3288-2517; Sabatini, Sabina/0000-0003-2076-5767; Caraveo, Patrizia/0000-0003-2478-8018; Komin, Nukri/0000-0003-3280-0582; Bastieri, Denis/0000-0002-6954-8862; Omodei, Nicola/0000-0002-5448-7577; Reimer, Olaf/0000-0001-6953-1385; Funk, Stefan/0000-0002-2012-0080; Gargano, Fabio/0000-0002-5055-6395; Johannesson, Gudlaugur/0000-0003-1458-7036; Loparco, Francesco/0000-0002-1173-5673; Moskalenko, Igor/0000-0001-6141-458X; Mazziotta, Mario /0000-0001-9325-4672; Bissaldi, Elisabetta/0000-0001-9935-8106; Torres, Diego/0000-0002-1522-9065; Rando, Riccardo/0000-0001-6992-818X; giglietto, nicola/0000-0002-9021-2888; Starck, Jean-Luc/0000-0003-2177-7794; Thompson, David/0000-0001-5217-9135; lubrano, pasquale/0000-0003-0221-4806; Morselli, Aldo/0000-0002-7704-9553 NR 203 TC 1445 Z9 1456 U1 31 U2 126 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 JUN 1 PY 2009 VL 697 IS 2 BP 1071 EP 1102 DI 10.1088/0004-637X/697/2/1071 PG 32 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 446YT UT WOS:000266159500012 ER PT J AU Koutroumpa, D Collier, MR Kuntz, KD Lallement, R Snowden, SL AF Koutroumpa, D. Collier, M. R. Kuntz, K. D. Lallement, R. Snowden, S. L. TI SOLAR WIND CHARGE EXCHANGE EMISSION FROM THE HELIUM FOCUSING CONE: MODEL TO DATA COMPARISON SO ASTROPHYSICAL JOURNAL LA English DT Article DE solar wind; X-rays: general ID X-RAY-EMISSION; NEUTRAL ATOMS; LOCAL BUBBLE; PICKUP IONS; XMM-NEWTON; 1 AU; INTERSTELLAR; HELIOSPHERE; PARAMETERS; CYCLE AB A model for heliospheric solar wind charge exchange (SWCX) X-ray emission is applied to a series of XMM-Newton observations of the interplanetary focusing cone of interstellar helium. The X-ray data are from three coupled observations of the South Ecliptic Pole (SEP; to observe the cone) and the Hubble Deep Field-North (HDF-N, to monitor global variations of the SWCX emission due to variations in the solar wind (SW)) from the period 2003 November 24 to December 15. There is good qualitative agreement between the model predictions and the data, after the SEP data are corrected using the HDF-N data, with the maximum SWCX flux observed at an ecliptic longitude of similar to 72 degrees, consistent with the central longitude of the He cone. We observe a total excess of 2.1 +/- 1.3 line unit (LU) in the O VII line and 2.0 +/- 0.9 LU in the O VIII line. However, the SWCX emission model, which was adjusted for SW conditions appropriate for late 2003, predicts an excess from the He cone of only 0.5 LU and 0.2 LU, respectively, in the O VII and O VIII lines. We discuss the model to data comparison and provide possible explanations for the discrepancies. We also qualitatively re-examine our SWCX model predictions in the 1/4 keV band with data from the ROSAT All-Sky Survey toward the North Ecliptic Pole and SEP, when the He cone was probably first detected in soft X-rays. C1 [Koutroumpa, D.; Collier, M. R.; Snowden, S. L.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Koutroumpa, D.; Lallement, R.] Univ Versailles St Quentin, CNRS, Serv Aeron, UMR 7620, F-91371 Verrieres Le Buisson, France. [Kuntz, K. D.] Johns Hopkins Univ, Henry A Rowland Dept Phys & Astron, Baltimore, MD 21218 USA. RP Koutroumpa, D (reprint author), NASA, Goddard Space Flight Ctr, Code 662, Greenbelt, MD 20771 USA. RI Snowden, Steven/D-5292-2012; Collier, Michael/I-4864-2013 OI Collier, Michael/0000-0001-9658-6605 FU NASA FX This research was supported by an appointment to the NASA Postdoctoral Program at the Goddard Space Flight Center, administered by Oak Ridge Associated Universities through a contract with NASA. NR 42 TC 21 Z9 21 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUN 1 PY 2009 VL 697 IS 2 BP 1214 EP 1225 DI 10.1088/0004-637X/697/2/1214 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 446YT UT WOS:000266159500023 ER PT J AU Serabyn, E AF Serabyn, E. TI HIGH-CONTRAST, NARROW-FIELD EXOPLANET IMAGING WITH A MULTI-APERTURE TELESCOPE PHASED-ARRAY CORONAGRAPH SO ASTROPHYSICAL JOURNAL LA English DT Article DE techniques: high angular resolution ID BAND PHASING ALGORITHM; EARTH-LIKE PLANETS; INTERFEROMETRIC ARRAYS; KECK TELESCOPES; MIRROR SEGMENTS; EXTRASOLAR; SYSTEM; LIMITS; FIBER AB The coronagraphic imaging of nearby solar systems with a densely packed array of small, inexpensive collector telescopes is considered. A reduced-scale segmented pupil can be assembled downstream of the collectors either by means of an array of delay lines, or more conveniently, by means of an array of single-mode fibers. In either case, the individual pupil elements are completely decoupled from each other. Tuning the intensity and phase of the light in each pupil element then allows complete control over the pupil-plane field, thus enabling arbitrary and tunable complex pupil-plane apodization. Calculations show that such a "phased-array coronagraph" (PAC) can in principle provide the 10(-10) image-plane contrast required for terrestrial exoplanet observations near bright stars. A PAC may thus provide a route to coronagraphic observations of faint exoplanets that is both flexible and potentially relatively inexpensive. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Serabyn, E (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr,MS 171-113, Pasadena, CA 91109 USA. EM gene.serabyn@jpl.nasa.gov FU Jet Propulsion Laboratory (JPL), California Institute of Technology; National Aeronautics and Space Administration FX The research described herein was carried out at the Jet Propulsion Laboratory ( JPL), California Institute of Technology, under a contract with the National Aeronautics and Space Administration. I thank S. R. Martin, K. Liewer, A. Ksendzov, and other colleagues at JPL for stimulating discussions of this idea, and the referee for numerous comments that led to a much improved paper. NR 25 TC 3 Z9 3 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUN 1 PY 2009 VL 697 IS 2 BP 1334 EP 1340 DI 10.1088/0004-637X/697/2/1334 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 446YT UT WOS:000266159500033 ER PT J AU Lynch, BJ Antiochos, SK Li, Y Luhmann, JG DeVore, CR AF Lynch, B. J. Antiochos, S. K. Li, Y. Luhmann, J. G. DeVore, C. R. TI ROTATION OF CORONAL MASS EJECTIONS DURING ERUPTION SO ASTROPHYSICAL JOURNAL LA English DT Article DE Sun: corona; Sun: coronal mass ejections (CMEs); Sun: magnetic fields ID MAGNETIC-FLUX TUBES; SOLAR-WIND; KINK INSTABILITY; ROPE STRUCTURE; NEUTRAL LINES; ACTIVE-REGION; CLOUDS; FIELDS; PROMINENCES; FILAMENTS AB Understanding the connection between coronal mass ejections (CMEs) and their interplanetary counterparts (ICMEs) is one of the most important problems in solar-terrestrial physics. We calculate the rotation of erupting field structures predicted by numerical simulations of CME initiation via the magnetic breakout model. In this model, the initial potential magnetic field has a multipolar topology and the system is driven by imposing a shear flow at the photospheric boundary. Our results yield insight on how to connect solar observations of the orientation of the filament or polarity inversion line (PIL) in the CME source region, the orientation of the CME axis as inferred from coronagraph images, and the ICME flux rope orientation obtained from in situ measurements. We present the results of two numerical simulations that differ only in the direction of the applied shearing motions (i.e., the handedness of the sheared-arcade systems and their resulting CME fields). In both simulations, eruptive flare reconnection occurs underneath the rapidly expanding sheared fields transforming the ejecta fields into three-dimensional flux rope structures. As the erupting flux ropes propagate through the low corona (from 2 to 4 R(circle dot)) the right-handed breakout flux rope rotates clockwise and the left-handed breakout flux rope rotates counterclockwise, in agreement with recent observations of the rotation of erupting filaments. We find that by 3.5 R(circle dot) the average rotation angle between the flux rope axes and the active region PIL is approximately 50 degrees. We discuss the implications of these results for predicting, from the observed chirality of the pre-eruption filament and/or other properties of the CME source region, the direction and amount of rotation that magnetic flux rope structures will experience during eruption. We also discuss the implications of our results for CME initiation models. C1 [Lynch, B. J.; Li, Y.; Luhmann, J. G.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Antiochos, S. K.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [DeVore, C. R.] USN, Res Lab, Computat Phys & Fluid Dynam Lab, Washington, DC 20375 USA. RP Lynch, BJ (reprint author), Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. EM blynch@ssl.berkeley.edu; spiro.k.antiochos@nasa.gov; yanli@ssl.berkeley.edu; jgluhman@ssl.berkeley.edu; devore@lcp.nrl.navy.mil RI Antiochos, Spiro/D-4668-2012; Lynch, Benjamin/B-1300-2013; DeVore, C/A-6067-2015; OI Antiochos, Spiro/0000-0003-0176-4312; DeVore, C/0000-0002-4668-591X; Lynch, Benjamin/0000-0001-6886-855X FU NSF [ATM-0621725]; NASA [NNX08AJ04G]; NASA HTP; SRT Programs; Office of Naval Research (ONR); SSL/UCB participation in the Center for Integrated Space-Weather Modeling (CISM) Collaboration FX B. J. L. gratefully acknowledges grants NSF SHINE ATM-0621725 and NASA HGI NNX08AJ04G. Additional support for this work comes from the NASA HTP and SR&T Programs, the Office of Naval Research (ONR), and SSL/UCB participation in the Center for Integrated Space-Weather Modeling (CISM) Collaboration. The DoD High Performance Computing Modernization Program provided resources at the ERDC major shared resource and NRL-DC distributed computing centers for this research. NR 71 TC 52 Z9 53 U1 0 U2 6 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUN 1 PY 2009 VL 697 IS 2 BP 1918 EP 1927 DI 10.1088/0004-637X/697/2/1918 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 446YT UT WOS:000266159500074 ER PT J AU Rauch, BF Link, JT Lodders, K Israel, MH Barbier, LM Binns, WR Christian, ER Cummings, JR de Nolfo, GA Geier, S Mewaldt, RA Mitchell, JW Schindler, SM Scott, LM Stone, EC Streitmatter, RE Waddington, CJ Wiedenbeck, ME AF Rauch, B. F. Link, J. T. Lodders, K. Israel, M. H. Barbier, L. M. Binns, W. R. Christian, E. R. Cummings, J. R. de Nolfo, G. A. Geier, S. Mewaldt, R. A. Mitchell, J. W. Schindler, S. M. Scott, L. M. Stone, E. C. Streitmatter, R. E. Waddington, C. J. Wiedenbeck, M. E. TI COSMIC RAY ORIGIN IN OB ASSOCIATIONS AND PREFERENTIAL ACCELERATION OF REFRACTORY ELEMENTS: EVIDENCE FROM ABUNDANCES OF ELEMENTS Fe-26 THROUGH Se-34 SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmic rays; Galaxy: abundances; ISM: abundances; stars: winds, outflows ID ISOTOPIC COMPOSITION; SUPERBUBBLE ORIGIN; SUPERNOVA-REMNANTS; CROSS-SECTIONS; MASSIVE STARS; NUCLEI; NEON; CHARGE; NUCLEOSYNTHESIS; HYDROGEN AB We report abundances of elements from Fe-26 to Se-34 in the cosmic radiation measured during fifty days of exposure of the Trans-Iron Galactic Element Recorder (TIGER) balloon-borne instrument. These observations add support to the concept that the bulk of cosmic ray acceleration takes place in OB associations, and they further support cosmic ray acceleration models in which elements present in interstellar grains are accelerated preferentially compared with those found in interstellar gas. C1 [Rauch, B. F.; Link, J. T.; Lodders, K.; Israel, M. H.; Binns, W. R.; Cummings, J. R.; Scott, L. M.] Washington Univ, St Louis, MO 63130 USA. [Link, J. T.; de Nolfo, G. A.] NASA, Goddard Space Flight Ctr, CRESST, Greenbelt, MD 20771 USA. [Geier, S.; Mewaldt, R. A.; Schindler, S. M.; Stone, E. C.] CALTECH, Pasadena, CA 91125 USA. [Waddington, C. J.] Univ Minnesota, Minneapolis, MN 55455 USA. [Wiedenbeck, M. E.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Rauch, BF (reprint author), Washington Univ, St Louis, MO 63130 USA. EM mhi@wustl.edu RI Christian, Eric/D-4974-2012; de Nolfo, Georgia/E-1500-2012 OI Christian, Eric/0000-0003-2134-3937; FU NASA at Washington University [NNG05WC04G]; Goddard Space Flight Center; California Institute of Technology [NNG05WC21G]; Caltech's Jet Propulsion Laboratory; NSF [AST0807356] FX We gratefully acknowledge the excellent work of the staff of the Columbia Scientific Balloon Facility, the NASA Balloon Program Office, and the NSF Office of Polar Programs who together made possible two successful long-duration balloon flights over Antarctica. This research was supported by NASA at Washington University (grant NNG05WC04G), Goddard Space Flight Center, the California Institute of Technology (grant NNG05WC21G), and Caltech's Jet Propulsion Laboratory. K.L.'s participation at Washington University was supported by the NSF (grant AST0807356). NR 43 TC 29 Z9 29 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 JUN 1 PY 2009 VL 697 IS 2 BP 2083 EP 2088 DI 10.1088/0004-637X/697/2/2083 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 446YT UT WOS:000266159500085 ER PT J AU Sargent, BA Forrest, WJ Tayrien, C McClure, MK Watson, DM Sloan, GC Li, A Manoj, P Bohac, CJ Furlan, E Kim, KH Green, JD AF Sargent, B. A. Forrest, W. J. Tayrien, C. McClure, M. K. Watson, Dan M. Sloan, G. C. Li, A. Manoj, P. Bohac, C. J. Furlan, E. Kim, K. H. Green, J. D. TI DUST PROCESSING AND GRAIN GROWTH IN PROTOPLANETARY DISKS IN THE TAURUS-AURIGA STAR-FORMING REGION SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Review DE circumstellar matter; infrared: stars; planetary systems: protoplanetary disks; stars: pre-main sequence ID INTERSTELLAR SILICATE MINERALOGY; SPITZER-SPACE-TELESCOPE; INFRARED-ABSORPTION SPECTRA; COMET HALE-BOPP; YOUNG CIRCUMSTELLAR DISKS; LARGE-MAGELLANIC-CLOUD; WATER ICE GROWTH; T-TAURI; CRYSTALLINE SILICATES; OPTICAL-PROPERTIES AB Mid-infrared spectra of 65 T Tauri stars (TTS) taken with the Infrared Spectrograph (IRS) on board the Spitzer Space Telescope are modeled using populations of optically thin warm and cool grains to probe the radial variation in dust composition in the uppermost layers of protoplanetary disks. Most spectra with narrow emission features associated with crystalline silicates require Mg-rich minerals and silica, while a few spectra with these features suggest the presence of other components. IRS spectra indicating the presence of large amounts of warm enstatite of similar to 400-500 K require crystalline silicates (enstatite or forsterite) at temperatures lower than the median temperature of the cool dust in the models, similar to 127 K; spectra showing a high abundance of other crystalline silicates (forsterite or silica) typically do not. A few spectra show 10 mu m complexes of very small equivalent width. They are fit well using abundant crystalline silicates but very few large grains, inconsistent with the expectation that a low peak-to-continuum ratio of the 10 mu m complex always indicates grain growth. Most of the spectra in our sample are fit well without using the opacities of large crystalline silicate grains. If large grains grow by agglomeration of submicron grains of all dust types, the amorphous silicate components of these aggregates must typically be more abundant than the crystalline silicate components. We also find that the more there is of one crystalline dust species, the more there is of the others. This could suggest that crystalline silicates are processed directly from amorphous silicates, whether through evaporation of the amorphous grains and condensation in chemical equilibrium or by annealing of the amorphous precursors. Alternatively, if one kind of crystalline silicate transforms into another kind, it suggests that the intermediate species transforms into the end-product species at a slower rate than the precursor transforms into the intermediate species; otherwise, there would be a negligible abundance of intermediate species. It is also found that the crystalline silicate abundance is correlated tightly with disk geometry, in the sense of higher crystallinity accompanying more-settled disks, which are commonly associated with growth and settling of grains. The abundance of large grains is also correlated with disks that are more highly settled, but with a wide range of large grain abundance for a given degree of settling. We interpret this range as that the settling of large grains is sensitive to individual disk properties. We also find that lower-mass stars have higher abundances of large grains in their inner regions. C1 [Sargent, B. A.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Forrest, W. J.; Tayrien, C.; Watson, Dan M.; Manoj, P.; Bohac, C. J.; Kim, K. H.; Green, J. D.] Univ Rochester, Dept Phys & Astron, Rochester, NY 14627 USA. [McClure, M. K.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Sloan, G. C.] Cornell Univ, Ctr Radiophys & Space Res, Ithaca, NY 14853 USA. [Li, A.] Univ Missouri, Dept Phys & Astron, Columbia, MO 65211 USA. [Furlan, E.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Sargent, BA (reprint author), Space Telescope Sci Inst, 3700 San Martin Dr, Baltimore, MD 21218 USA. EM sargent@stsci.edu OI McClure, Melissa/0000-0003-1878-327X; Furlan, Elise/0000-0001-9800-6248 NR 123 TC 67 Z9 68 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0067-0049 J9 ASTROPHYS J SUPPL S JI Astrophys. J. Suppl. Ser. PD JUN PY 2009 VL 182 IS 2 BP 477 EP 508 DI 10.1088/0067-0049/182/2/477 PG 32 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 448UE UT WOS:000266286700001 ER PT J AU Abazajian, KN Adelman-McCarthy, JK Agueros, MA Allam, SS Prieto, CA An, D Anderson, KSJ Anderson, SF Annis, J Bahcall, NA Bailer-Jones, CAL Barentine, JC Bassett, BA Becker, AC Beers, TC Bell, EF Belokurov, V Berlind, AA Berman, EF Bernardi, M Bickerton, SJ Bizyaev, D Blakeslee, JP Blanton, MR Bochanski, JJ Boroski, WN Brewington, HJ Brinchmann, J Brinkmann, J Brunner, RJ Budavari, T Carey, LN Carliles, S Carr, MA Castander, FJ Cinabro, D Connolly, AJ Csabai, I Cunha, CE Czarapata, PC Davenport, JRA de Haas, E Dilday, B Doi, M Eisenstein, DJ Evans, ML Evans, NW Fan, XH Friedman, SD Frieman, JA Fukugita, M Gansicke, BT Gates, E Gillespie, B Gilmore, G Gonzalez, B Gonzalez, CF Grebel, EK Gunn, JE Gyory, Z Hall, PB Harding, P Harris, FH Harvanek, M Hawley, SL Hayes, JJE Heckman, TM Hendry, JS Hennessy, GS Hindsley, RB Hoblitt, J Hogan, CJ Hogg, DW Holtzman, JA Hyde, JB Ichikawa, S Ichikawa, T Im, M Ivezic, Z Jester, S Jiang, LH Johnson, JA Jorgensen, AM Juric, M Kent, SM Kessler, R Kleinman, SJ Knapp, GR Konishi, K Kron, RG Krzesinski, J Kuropatkin, N Lampeitl, H Lebedeva, S Lee, MG Lee, YS Leger, RF Lepine, S Li, NL Lima, M Lin, H Long, DC Loomis, CP Loveday, J Lupton, RH Magnier, E Malanushenko, O Malanushenko, V Mandelbaum, R Margon, B Marriner, JP Martinez-Delgado, D Matsubara, T McGehee, PM McKay, TA Meiksin, A Morrison, HL Mullally, F Munn, JA Murphy, T Nash, T Nebot, A Neilsen, EH Newberg, HJ Newman, PR Nichol, RC Nicinski, T Nieto-Santisteban, M Nitta, A Okamura, S Oravetz, DJ Ostriker, JP Owen, R Padmanabhan, N Pan, KK Park, C Pauls, G Peoples, J Percival, WJ Pier, JR Pope, AC Pourbaix, D Price, PA Purger, N Quinn, T Raddick, MJ Fiorentin, PR Richards, GT Richmond, MW Riess, AG Rix, HW Rockosi, CM Sako, M Schlegel, DJ Schneider, DP Scholz, RD Schreiber, MR Schwope, AD Seljak, U Sesar, B Sheldon, E Shimasaku, K Sibley, VC Simmons, AE Sivarani, T Smith, JA Smith, MC Smolcic, V Snedden, SA Stebbins, A Steinmetz, M Stoughton, C Strauss, MA SubbaRao, M Suto, Y Szalay, AS Szapudi, I Szkody, P Tanaka, M Tegmark, M Teodoro, LFA Thakar, AR Tremonti, CA Tucker, DL Uomoto, A Berk, DEV Vandenberg, J Vidrih, S Vogeley, MS Voges, W Vogt, NP Wadadekar, Y Watters, S Weinberg, DH West, AA White, SDM Wilhite, BC Wonders, AC Yanny, B Yocum, DR York, DG Zehavi, I Zibetti, S Zucker, DB AF Abazajian, Kevork N. Adelman-McCarthy, Jennifer K. Agueros, Marcel A. Allam, Sahar S. Prieto, Carlos Allende An, Deokkeun Anderson, Kurt S. J. Anderson, Scott F. Annis, James Bahcall, Neta A. Bailer-Jones, C. A. L. Barentine, J. C. Bassett, Bruce A. Becker, Andrew C. Beers, Timothy C. Bell, Eric F. Belokurov, Vasily Berlind, Andreas A. Berman, Eileen F. Bernardi, Mariangela Bickerton, Steven J. Bizyaev, Dmitry Blakeslee, John P. Blanton, Michael R. Bochanski, John J. Boroski, William N. Brewington, Howard J. Brinchmann, Jarle Brinkmann, J. Brunner, Robert J. Budavari, Tamas Carey, Larry N. Carliles, Samuel Carr, Michael A. Castander, Francisco J. Cinabro, David Connolly, A. J. Csabai, Istvan Cunha, Carlos E. Czarapata, Paul C. Davenport, James R. A. de Haas, Ernst Dilday, Ben Doi, Mamoru Eisenstein, Daniel J. Evans, Michael L. Evans, N. W. Fan, Xiaohui Friedman, Scott D. Frieman, Joshua A. Fukugita, Masataka Gansicke, Boris T. Gates, Evalyn Gillespie, Bruce Gilmore, G. Gonzalez, Belinda Gonzalez, Carlos F. Grebel, Eva K. Gunn, James E. Gyory, Zsuzsanna Hall, Patrick B. Harding, Paul Harris, Frederick H. Harvanek, Michael Hawley, Suzanne L. Hayes, Jeffrey J. E. Heckman, Timothy M. Hendry, John S. Hennessy, Gregory S. Hindsley, Robert B. Hoblitt, J. Hogan, Craig J. Hogg, David W. Holtzman, Jon A. Hyde, Joseph B. Ichikawa, Shin-ichi Ichikawa, Takashi Im, Myungshin Ivezic, Zeljko Jester, Sebastian Jiang, Linhua Johnson, Jennifer A. Jorgensen, Anders M. Juric, Mario Kent, Stephen M. Kessler, R. Kleinman, S. J. Knapp, G. R. Konishi, Kohki Kron, Richard G. Krzesinski, Jurek Kuropatkin, Nikolay Lampeitl, Hubert Lebedeva, Svetlana Lee, Myung Gyoon Lee, Young Sun Leger, R. French Lepine, Sebastien Li, Nolan Lima, Marcos Lin, Huan Long, Daniel C. Loomis, Craig P. Loveday, Jon Lupton, Robert H. Magnier, Eugene Malanushenko, Olena Malanushenko, Viktor Mandelbaum, Rachel Margon, Bruce Marriner, John P. Martinez-Delgado, David Matsubara, Takahiko McGehee, Peregrine M. McKay, Timothy A. Meiksin, Avery Morrison, Heather L. Mullally, Fergal Munn, Jeffrey A. Murphy, Tara Nash, Thomas Nebot, Ada Neilsen, Eric H., Jr. Newberg, Heidi Jo Newman, Peter R. Nichol, Robert C. Nicinski, Tom Nieto-Santisteban, Maria Nitta, Atsuko Okamura, Sadanori Oravetz, Daniel J. Ostriker, Jeremiah P. Owen, Russell Padmanabhan, Nikhil Pan, Kaike Park, Changbom Pauls, George Peoples, John, Jr. Percival, Will J. Pier, Jeffrey R. Pope, Adrian C. Pourbaix, Dimitri Price, Paul A. Purger, Norbert Quinn, Thomas Raddick, M. Jordan Fiorentin, Paola Re Richards, Gordon T. Richmond, Michael W. Riess, Adam G. Rix, Hans-Walter Rockosi, Constance M. Sako, Masao Schlegel, David J. Schneider, Donald P. Scholz, Ralf-Dieter Schreiber, Matthias R. Schwope, Axel D. Seljak, Uros Sesar, Branimir Sheldon, Erin Shimasaku, Kazu Sibley, Valena C. Simmons, A. E. Sivarani, Thirupathi Smith, J. Allyn Smith, Martin C. Smolcic, Vernesa Snedden, Stephanie A. Stebbins, Albert Steinmetz, Matthias Stoughton, Chris Strauss, Michael A. SubbaRao, Mark Suto, Yasushi Szalay, Alexander S. Szapudi, Istvan Szkody, Paula Tanaka, Masayuki Tegmark, Max Teodoro, Luis F. A. Thakar, Aniruddha R. Tremonti, Christy A. Tucker, Douglas L. Uomoto, Alan Berk, Daniel E. Vanden Vandenberg, Jan Vidrih, S. Vogeley, Michael S. Voges, Wolfgang Vogt, Nicole P. Wadadekar, Yogesh Watters, Shannon Weinberg, David H. West, Andrew A. White, Simon D. M. Wilhite, Brian C. Wonders, Alainna C. Yanny, Brian Yocum, D. R. York, Donald G. Zehavi, Idit Zibetti, Stefano Zucker, Daniel B. TI THE SEVENTH DATA RELEASE OF THE SLOAN DIGITAL SKY SURVEY SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE atlases; catalogs; surveys ID SPECTROSCOPIC TARGET SELECTION; CCD ASTROGRAPH CATALOG; GALAXY SAMPLE; OPEN CLUSTERS; STARS; PHOTOMETRY; SYSTEM; FIELD; CALIBRATION; MANAGEMENT AB This paper describes the Seventh Data Release of the Sloan Digital Sky Survey (SDSS), marking the completion of the original goals of the SDSS and the end of the phase known as SDSS-II. It includes 11,663 deg(2) of imaging data, with most of the similar to 2000 deg(2) increment over the previous data release lying in regions of low Galactic latitude. The catalog contains five-band photometry for 357 million distinct objects. The survey also includes repeat photometry on a 120 degrees long, 2 degrees.5 wide stripe along the celestial equator in the Southern Galactic Cap, with some regions covered by as many as 90 individual imaging runs. We include a co-addition of the best of these data, going roughly 2 mag fainter than the main survey over 250 deg(2). The survey has completed spectroscopy over 9380 deg(2); the spectroscopy is now complete over a large contiguous area of the Northern Galactic Cap, closing the gap that was present in previous data releases. There are over 1.6 million spectra in total, including 930,000 galaxies, 120,000 quasars, and 460,000 stars. The data release includes improved stellar photometry at low Galactic latitude. The astrometry has all been recalibrated with the second version of the USNO CCD Astrograph Catalog, reducing the rms statistical errors at the bright end to 45 milliarcseconds per coordinate. We further quantify a systematic error in bright galaxy photometry due to poor sky determination; this problem is less severe than previously reported for the majority of galaxies. Finally, we describe a series of improvements to the spectroscopic reductions, including better flat fielding and improved wavelength calibration at the blue end, better processing of objects with extremely strong narrow emission lines, and an improved determination of stellar metallicities. C1 [Abazajian, Kevork N.] Univ Maryland, Dept Phys, College Pk, MD 20742 USA. [Adelman-McCarthy, Jennifer K.; Allam, Sahar S.; Annis, James; Berman, Eileen F.; Boroski, William N.; Czarapata, Paul C.; Frieman, Joshua A.; Gonzalez, Belinda; Gonzalez, Carlos F.; Hendry, John S.; Hogan, Craig J.; Kent, Stephen M.; Kron, Richard G.; Kuropatkin, Nikolay; Lebedeva, Svetlana; Lin, Huan; Marriner, John P.; Nash, Thomas; Neilsen, Eric H., Jr.; Nicinski, Tom; Peoples, John, Jr.; Sibley, Valena C.; Stebbins, Albert; Stoughton, Chris; Tucker, Douglas L.; Yanny, Brian; Yocum, D. R.] Fermilab Natl Accelerator Lab, Batavia, IL 60510 USA. [Agueros, Marcel A.] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA. [Allam, Sahar S.] Univ Wyoming, Dept Phys & Astron, Laramie, WY 82071 USA. [Prieto, Carlos Allende] Univ Coll London, Mullard Space Sci Lab, Holmbury Sl Mary RH5 6NT, Surrey, England. [An, Deokkeun; Johnson, Jennifer A.; Weinberg, David H.] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA. [An, Deokkeun; McGehee, Peregrine M.] CALTECH, IPAC, Pasadena, CA 91125 USA. [Anderson, Kurt S. J.; Bizyaev, Dmitry; Brewington, Howard J.; Brinkmann, J.; Krzesinski, Jurek; Long, Daniel C.; Malanushenko, Olena; Malanushenko, Viktor; Newman, Peter R.; Oravetz, Daniel J.; Pan, Kaike; Simmons, A. E.; Snedden, Stephanie A.; Watters, Shannon] Apache Point Observ, Sunspot, NM 88349 USA. [Anderson, Kurt S. J.; Holtzman, Jon A.; Vogt, Nicole P.] New Mexico State Univ, Dept Astron, Las Cruces, NM 88003 USA. [Anderson, Scott F.; Becker, Andrew C.; Bochanski, John J.; Carey, Larry N.; Connolly, A. J.; Evans, Michael L.; Hawley, Suzanne L.; Ivezic, Zeljko; Leger, R. French; Owen, Russell; Quinn, Thomas; Sesar, Branimir; Stoughton, Chris; Szkody, Paula] Univ Washington, Dept Astron, Seattle, WA 98195 USA. [Bahcall, Neta A.; Bickerton, Steven J.; Carr, Michael A.; Gunn, James E.; Knapp, G. R.; Loomis, Craig P.; Lupton, Robert H.; Mullally, Fergal; Ostriker, Jeremiah P.; Pauls, George; Pourbaix, Dimitri; Strauss, Michael A.; Wadadekar, Yogesh] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. [Bailer-Jones, C. A. L.; Bell, Eric F.; Jester, Sebastian; Fiorentin, Paola Re; Rix, Hans-Walter; Tremonti, Christy A.; Zibetti, Stefano] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Barentine, J. C.] Univ Texas Austin, McDonald Observ, Austin, TX 78712 USA. [Barentine, J. C.] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA. [Bassett, Bruce A.] S African Astron Observ, ZA-7935 Cape Town, South Africa. [Bassett, Bruce A.] Univ Cape Town, ZA-7925 Cape Town, South Africa. [Beers, Timothy C.; Lee, Young Sun; Sivarani, Thirupathi] Michigan State Univ, CSCE, Dept Phys & Astrophys, E Lansing, MI 48824 USA. [Beers, Timothy C.; Sivarani, Thirupathi] Michigan State Univ, JINA, E Lansing, MI 48824 USA. [Belokurov, Vasily; Evans, N. W.; Gilmore, G.; Smith, Martin C.; Zucker, Daniel B.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. [Berlind, Andreas A.] Vanderbilt Univ, Dept Phys & Astron, Nashville, TN 37235 USA. [Bernardi, Mariangela; Hyde, Joseph B.; Lima, Marcos; Sako, Masao] Univ Penn, Dept Phys & Astron, Philadelphia, PA 19104 USA. [Blakeslee, John P.] Natl Res Council Canada, Herzberg Inst Astrophys, Victoria, BC V9E 2E7, Canada. [Blanton, Michael R.; Hogg, David W.; Sheldon, Erin] NYU, Dept Phys, Ctr Cosmol & Particle Phys, New York, NY 10003 USA. [Bochanski, John J.; West, Andrew A.] MIT Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. [Brinchmann, Jarle] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. 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A.] San Diego State Univ, Dept Astron, San Diego, CA 92182 USA. [de Haas, Ernst] Princeton Univ, Joseph Henry Labs, Princeton, NJ 08544 USA. [Dilday, Ben; Lima, Marcos] Univ Chicago, Dept Phys, Chicago, IL 60637 USA. [Dilday, Ben; Frieman, Joshua A.; Gates, Evalyn; Kessler, R.; Lima, Marcos] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA. [Dilday, Ben] Rutgers State Univ, Dept Phys & Astron, Piscataway, NJ 08854 USA. [Doi, Mamoru] Univ Tokyo, Grad Sch Sci, Inst Astron, Mitaka, Tokyo 1810015, Japan. [Doi, Mamoru] Univ Tokyo, Inst Phys & Math Universe, Kashiwa, Chiba 2778568, Japan. [Eisenstein, Daniel J.; Fan, Xiaohui; Jiang, Linhua] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Friedman, Scott D.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Frieman, Joshua A.; Kron, Richard G.; SubbaRao, Mark; York, Donald G.] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA. [Fukugita, Masataka; Konishi, Kohki] Univ Tokyo, Inst Cosm Ray Res, Kashiwa, Chiba 2778582, Japan. [Gansicke, Boris T.] Univ Warwick, Dept Phys, Coventry CV4 7AL, W Midlands, England. [Grebel, Eva K.; Vidrih, S.] Univ Heidelberg, Zentrum Astron, Astron Rech Inst, D-69120 Heidelberg, Germany. [Hall, Patrick B.] York Univ, Dept Phys & Astron, Toronto, ON M3J 1P3, Canada. [Harding, Paul; Morrison, Heather L.; Zehavi, Idit] Case Western Reserve Univ, Dept Astron, Cleveland, OH 44106 USA. [Harris, Frederick H.; Munn, Jeffrey A.; Pier, Jeffrey R.] USN Observ, Flagstaff Stn, Flagstaff, AZ 86001 USA. [Harvanek, Michael] Lowell Observ, Flagstaff, AZ 86001 USA. [Hayes, Jeffrey J. E.] NASA Headquarters, Heliophys Div, Sci Mission Directorate, Washington, DC 20546 USA. [Hennessy, Gregory S.] USN Observ, Washington, DC 20392 USA. [Hindsley, Robert B.] USN, Remote Sensing Div, Res Lab, Washington, DC 20392 USA. 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[Krzesinski, Jurek] Akad Pedog Krakowie, Obserwatorium Astron Suhorze, PL-30084 Krakow, Poland. [Lampeitl, Hubert; Nichol, Robert C.; Percival, Will J.] Univ Portsmouth, ICG, Portsmouth PO1 2EG, Hants, England. [Lepine, Sebastien] Amer Museum Nat Hist, Dept Astrophys, New York, NY 10024 USA. [Loveday, Jon] Univ Sussex, Ctr Astron, Brighton BN1 9QH, E Sussex, England. [Margon, Bruce] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA. [Martinez-Delgado, David] Inst Astrofis Canarias, E-38205 Tenerife, Spain. [Matsubara, Takahiko] Nagoya Univ, Dept Phys & Astrophys, Nagoya, Aichi 4648602, Japan. [Meiksin, Avery; Murphy, Tara] Univ Edinburgh, Royal Observ, Inst Astron, SUPA, Edinburgh EH9 3HJ, Midlothian, Scotland. [Murphy, Tara] Univ Sydney, Sydney Inst Astron, Sydney, NSW 2006, Australia. [Nebot, Ada; Scholz, Ralf-Dieter; Schwope, Axel D.; Steinmetz, Matthias] Astrophys Inst Potsdam, D-14482 Potsdam, Germany. [Newberg, Heidi Jo] Rensselaer Polytech Inst, Dept Phys Appl Phys & Astron, Troy, NY 12180 USA. [Newman, Peter R.; Nicinski, Tom] CMC Elect Aurora, Sugar Grove, IL 60554 USA. [Padmanabhan, Nikhil; Schlegel, David J.; Seljak, Uros] Lawrence Berkeley Natl Lab, Berkeley, CA 94720 USA. [Park, Changbom] Korea Inst Adv Study, Seoul 130722, South Korea. [Pope, Adrian C.] Los Alamos Natl Lab, Los Alamos, NM 87545 USA. [Pourbaix, Dimitri] Univ Libre Bruxelles, FNRS Inst Astron & Astrophys, B-1050 Brussels, Belgium. [Fiorentin, Paola Re] Univ Ljubljana, Dept Phys, Ljubljana 1000, Slovenia. [Richards, Gordon T.; Vogeley, Michael S.] Drexel Univ, Dept Phys, Philadelphia, PA 19104 USA. [Richmond, Michael W.] Rochester Inst Technol, Dept Phys, Rochester, NY 14623 USA. [Rockosi, Constance M.] Univ Calif Santa Cruz, Lick Observ, UCO, Santa Cruz, CA 95064 USA. [Sako, Masao] Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, Stanford, CA 94309 USA. [Schneider, Donald P.; Berk, Daniel E. Vanden] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Schreiber, Matthias R.] Univ Valparaiso, Dept Fis & Astron, Valparaiso, Chile. [Seljak, Uros] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA. [Seljak, Uros] Univ Zurich, Inst Theoret Phys, CH-8057 Zurich, Switzerland. [Sheldon, Erin] Brookhaven Natl Lab, Upton, NY 11973 USA. [Sivarani, Thirupathi] Univ Florida, Dept Astron, Bryant Space Sci Ctr, Gainesville, FL 32611 USA. [Smith, J. Allyn] Austin Peay State Univ, Dept Phys & Astron, Clarksville, TN 37040 USA. [SubbaRao, Mark] Adler Planetarium & Astron Museum, Chicago, IL 60605 USA. [Tanaka, Masayuki] European So Observ, D-85748 Garching, Germany. [Tegmark, Max] MIT, Dept Phys, Cambridge, MA 02139 USA. [Teodoro, Luis F. A.] Univ Glasgow, Dept Phys & Astron, Astron & Astrophys Grp, Glasgow G12 8QQ, Lanark, Scotland. [Uomoto, Alan] Observ Carnegie Inst Washington, Pasadena, CA 91101 USA. [Berk, Daniel E. Vanden] St Vincent Coll, Dept Phys, Latrobe, PA 15650 USA. [Voges, Wolfgang] Max Planck Inst Extraterr Phys, D-85741 Garching, Germany. [Wadadekar, Yogesh] Tata Inst Fundamental Res, Natl Ctr Radio Astrophys, Pune 411007, Maharashtra, India. [Watters, Shannon] Inst Astron, Adv Technol & Res Ctr, Pukalani, HI 96768 USA. [White, Simon D. M.] Max Planck Inst Astrophys, D-85748 Garching, Germany. [Wilhite, Brian C.] Elmhurst Coll, Dept Phys, Chicago, IL 60126 USA. [York, Donald G.] Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA. RP Abazajian, KN (reprint author), Univ Maryland, Dept Phys, College Pk, MD 20742 USA. RI Lima, Marcos/E-8378-2010; Padmanabhan, Nikhil/A-2094-2012; Gaensicke, Boris/A-9421-2012; Margon, Bruce/B-5913-2012; Csabai, Istvan/F-2455-2012; Im, Myungshin/B-3436-2013; McKay, Timothy/C-1501-2009; West, Andrew/H-3717-2014; Agueros, Marcel/K-7998-2014; Mandelbaum, Rachel/N-8955-2014; Brinchmann, Jarle/M-2616-2015; Jiang, Linhua/H-5485-2016; OI Murphy, Tara/0000-0002-2686-438X; Re Fiorentin, Paola/0000-0002-4995-0475; Meiksin, Avery/0000-0002-5451-9057; Csabai, Istvan/0000-0001-9232-9898; /0000-0002-1891-3794; Hogg, David/0000-0003-2866-9403; Davenport, James/0000-0002-0637-835X; Bell, Eric/0000-0002-5564-9873; Blakeslee, John/0000-0002-5213-3548; Gaensicke, Boris/0000-0002-2761-3005; Im, Myungshin/0000-0002-8537-6714; McKay, Timothy/0000-0001-9036-6150; Agueros, Marcel/0000-0001-7077-3664; Mandelbaum, Rachel/0000-0003-2271-1527; Brinchmann, Jarle/0000-0003-4359-8797; Jiang, Linhua/0000-0003-4176-6486; Tucker, Douglas/0000-0001-7211-5729 FU Alfred P. Sloan Foundation; National Science Foundation; U. S. Department of Energy; National Aeronautics and Space Administration; Japanese Monbukagakusho; Max Planck Society; Higher Education Funding Council for England FX Funding for the SDSS and SDSS-II has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation, the U. S. Department of Energy, the National Aeronautics and Space Administration, the Japanese Monbukagakusho, the Max Planck Society, and the Higher Education Funding Council for England. NR 73 TC 2563 Z9 2589 U1 26 U2 173 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0067-0049 J9 ASTROPHYS J SUPPL S JI Astrophys. J. Suppl. Ser. PD JUN PY 2009 VL 182 IS 2 BP 543 EP 558 DI 10.1088/0067-0049/182/2/543 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 448UE UT WOS:000266286700004 ER PT J AU Unger, N Shindell, DT Wang, JS AF Unger, Nadine Shindell, Drew T. Wang, James S. TI Climate forcing by the on-road transportation and power generation sectors SO ATMOSPHERIC ENVIRONMENT LA English DT Article DE Radiative forcing; Ozone; Aerosols; Transportation; Electric power; PHEV ID AIR-POLLUTION; REGIONAL EMISSIONS; BLACK CARBON; OZONE; SIMULATIONS; MORTALITY; FUEL; PREINDUSTRIAL; QUALITY AB The on-road transportation (ORT) and power generation (PG) sectors are major contributors to carbon dioxide (CO2) emissions and a host of short-lived radiatively-active air pollutants, including tropospheric ozone and fine aerosol particles, that exert complex influences on global climate. Effective mitigation of global climate change necessitates action in these sectors for which technology change options exist or are being developed. Most assessments of possible energy change options to date have neglected non-CO2 air pollutant impacts on radiative forcing (RF). In a multi-pollutant approach, we apply a global atmospheric composition-climate model to quantify the total RF from the global and United States (U.S.) ORT and PG sectors. We assess the RF for 2 time horizons: 20- and 100-year that are relevant for understanding near-term and longer-term impacts of climate change, respectively. ORT is a key target sector to mitigate global climate change because the net non-CO2 RF is positive and acts to enhance considerably the CO2 warming impacts. We perform further sensitivity studies to assess the RF impacts of a potential major technology shift that would reduce ORT emissions by 50% with the replacement energy supplied either by a clean zero-emissions source (S1) or by the PG sector, which results in an estimated 20% penalty increase in emissions from this sector (S2). We examine cases where the technology shift is applied globally and in the U.S. only. The resultant RF relative to the present day control is negative (cooling) in all cases for both S1 and S2 scenarios, global and U.S. emissions, and 20- and 100-year time horizons. The net non-CO2 RF is always important relative to the CO2 RF and outweighs the CO2 RF response in the S2 scenario for both time horizons. Assessment of the full impacts of technology and policy strategies designed to mitigate global climate change must consider the climate effects of ozone and fine aerosol particles. (C) 2009 Elsevier Ltd. All rights reserved. C1 [Unger, Nadine; Shindell, Drew T.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA. [Unger, Nadine] Columbia Univ, Ctr Climate Syst Res, New York, NY 10025 USA. [Wang, James S.] Environm Def Fund, New York, NY 10010 USA. RP Unger, N (reprint author), NASA, Goddard Inst Space Studies, New York, NY 10025 USA. EM nunger@giss.nasa.gov RI Shindell, Drew/D-4636-2012; Unger, Nadine/M-9360-2015 FU NASA Atmospheric Chemistry Modeling and Analysis Program; NASA Center for Computational Sciences FX This research is supported by the NASA Atmospheric Chemistry Modeling and Analysis Program. We thank the NASA Center for Computational Sciences for computing support. We thank T. Wigley and S. Raper for creating the MAGICC model and making it publicly available. NR 41 TC 21 Z9 21 U1 1 U2 12 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 JUN PY 2009 VL 43 IS 19 BP 3077 EP 3085 DI 10.1016/j.atmosenv.2009.03.021 PG 9 WC Environmental Sciences; Meteorology & Atmospheric Sciences SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences GA 457AE UT WOS:000266896000006 ER PT J AU Fairlie, TD Szykman, J Gilliland, A Pierce, RB Kittaka, C Weber, S Engel-Cox, J Rogers, RR Tikvart, J Scheffe, R Dimmick, F AF Fairlie, T. Duncan Szykman, James Gilliland, Alice Pierce, R. Bradley Kittaka, Chieko Weber, Stephanie Engel-Cox, Jill Rogers, Raymond R. Tikvart, Joe Scheffe, Rich Dimmick, Fred TI Lagrangian sampling of 3-D air quality model results for regional transport contributions to sulfate aerosol concentrations at Baltimore, MD, in summer 2004 SO ATMOSPHERIC ENVIRONMENT LA English DT Article DE Air quality; Source apportionment modeling; CAIR; CMAQ; Satellite; MODIS; Sulfate; Particulate matter ID FINE PARTICULATE MATTER; UNITED-STATES; OPTICAL DEPTH; TRENDS; VALIDATION; OZONE AB We use ensemble-mean Lagrangian sampling of a 3-D Eulerian air quality model, CMAQ together with ground-based ambient monitors data from several air monitoring networks and satellite (MODIS) observations to provide source apportionment and regional transport vs. local contributions to sulfate aerosol and PM2.5 concentrations at Baltimore, MD, for summer 2004. The Lagrangian method provides estimates of the chemical and physical evolution of air arriving in the daytime boundary layer at Baltimore. Study results indicate a dominant role for regional transport contributions on those days when sulfate air pollution is highest in Baltimore, with a principal transport pathway from the Ohio River Valley (ORV) through southern Pennsylvania and Maryland, consistent with earlier studies. Thus, reductions in sulfur emissions from the ORV under the EPA's Clean Air Interstate Rule may be expected to improve particulate air quality in Baltimore during summer. The Lagrangian sampling of CMAQ offers an inexpensive and complimentary approach to traditional methods of source apportionment based on multivariate observational data analysis, and air quality model emissions separation. This study serves as a prototype for the method applied to Baltimore. EPA is establishing a system to allow air quality planners to readily produce and access equivalent results for locations of their choice. Published by Elsevier Ltd. C1 [Fairlie, T. Duncan] US Natl Aeronaut & Space Adm, Langley Res Ctr, Sci Directorate, Hampton, VA 23681 USA. [Szykman, James; Gilliland, Alice; Dimmick, Fred] US EPA, Off Res & Dev, Natl Exposure Res Lab, Res Triangle Pk, NC 27711 USA. [Pierce, R. Bradley] Natl Environm Satellite Data & Informat Serv, Natl Ocean & Atmospher Adm, Madison, WI 53706 USA. [Kittaka, Chieko; Rogers, Raymond R.] Sci Applicat Int Corp SSAI, Hampton, VA 23666 USA. [Weber, Stephanie] Battelle Mem Inst, Columbus, OH 43201 USA. [Engel-Cox, Jill] Battelle Mem Inst, Arlington, VA 22201 USA. [Tikvart, Joe; Scheffe, Rich] US EPA, Off Air Qual Planning & Stand, Res Triangle Pk, NC 27711 USA. RP Fairlie, TD (reprint author), US Natl Aeronaut & Space Adm, Langley Res Ctr, Sci Directorate, Hampton, VA 23681 USA. EM t.d.fairlie@larc.nasa.gov RI Pierce, Robert Bradley/F-5609-2010; Wang, Linden/M-6617-2014 OI Pierce, Robert Bradley/0000-0002-2767-1643; FU NASA Applied Sciences Program; EPA FX We wish to thank Tanya Otte, Alfreida Torian, and colleagues at Research Triangle Park for providing the CMAQ model and MCIP meteorological fields used in this study. We thank CIMSS, University of Wisconsin, for use of the MODIS data. We thank the AERONET and IMPROVE science teams for use of their data. We thank Ray Hoff (UMBQ for use of the ELF data. Thanks to Matt Seybold (NOAA NESDIS), Mike Woodman (Maryland Department of Environment), and to Susan Wierman (Mid-Atlantic Regional Management Association - MARAMA) for reviews on this work. Thanks to Jeff Stehr (University of Maryland), and Dev Roy (US EPA) for their technical input and discussions, and to the anonymous reviewers of this manuscript for their comments and suggestions. We thank Lawrence Friedl and Doreen Neil for supporting this work through the NASA Applied Sciences Program. Additional support was provided by EPA through the EPA Global Earth Observation (GEO) Advance Monitoring Initiative (AMI). The views expressed and findings contained in this paper are those of the authors and should not be construed as official NASA, EPA, NOAA, or U.S. Government position, policy, or decision. NR 39 TC 12 Z9 13 U1 0 U2 7 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 JUN PY 2009 VL 43 IS 20 BP 3275 EP 3288 DI 10.1016/j.atmosenv.2009.02.026 PG 14 WC Environmental Sciences; Meteorology & Atmospheric Sciences SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences GA 459PY UT WOS:000267117100015 ER PT J AU Bearman, C Paletz, SBF Orasanu, J AF Bearman, Chris Paletz, Susannah B. F. Orasanu, Judith TI Situational Pressures on Aviation Decision Making: Goal Seduction and Situation Aversion SO AVIATION SPACE AND ENVIRONMENTAL MEDICINE LA English DT Article DE plan continuation errors; goal seduction; situation aversion; Alaska AB BEARMAN C, PALETZ SBF, ORASANU J. Situational pressures on aviation decision making. goal seduction and situation aversion. Aviat Space Environ Med 2009; 80:556-60. Introduction: The context in which a decision is made can shape the decision process in important ways. Of particular interest here are 'strong' situations, that is, contexts where the situation itself exerts an influence on decision making. Borrowing concepts from field theory and approach/avoidance theory, this paper explores the influence of strong situations on pilot decision making. Method: There were 28 pilots flying in Alaska who were interviewed using a critical incident technique where participants were asked to relate stories about challenging flying situations. A bottom-up qualitative analysis of reported social and psychological pressures revealed a range of types, including strong situations, which are described in this paper. Results: Strong situations were mentioned in 67% of the interviews and included situations likely to motivate the pilot toward unsafe behavior (goal seduction) and situations likely to motivate the pilot away from safe behavior (situation aversion). Goal seduction situations included rescuing others, meeting a significant other, time-related constraints, financial pressures, and unspecified goal seduction; aversive situations included physical discomfort, not having maintenance or facilities for the airplane, and a lack of basic necessities (e.g., lodging) for the pilot. Discussion: Goal seduction describes one broad, unspecified influence on pilot decision making, but situation aversion is also an important motivator for some pilots. Goal seduction and situation aversion may well underlie the phenomena of plan continuation errors, the tendency for pilots to continue despite evidence suggesting it is imprudent. This study suggests some specific factors that constrain decision making for pilots in challenging situations. C1 [Bearman, Chris] Univ S Australia, Adelaide, SA 5001, Australia. [Paletz, Susannah B. F.; Orasanu, Judith] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. EM chris.bearman@unisa.edu.au FU NASA; FAA's Office of Human Factors FX We Would like to thank Barbara Burian, Philip Lieberman, Jessica Nowinksi, and an anonymous reviewer for their helpful comments on this manuscript. We would also like to thank Jon Holbrook and C. Elaine McCoy for their professional contributions to the work and Jane Bearman, Wayne Daniels, Steve Farlow, Karen Wegienek, and members of the University of South Australia's Centre for Sleep Research for their limited technical or supporting roles in this project. This research was supported by NASA's Aviation Safety Program, the FAA's Office of Human Factors, and by an appointment to the first author to the NASA postdoctoral program at Ames Research Center, administered by Oak Ridge Associated Universities. NR 14 TC 8 Z9 8 U1 2 U2 8 PU AEROSPACE MEDICAL ASSOC PI ALEXANDRIA PA 320 S HENRY ST, ALEXANDRIA, VA 22314-3579 USA SN 0095-6562 J9 AVIAT SPACE ENVIR MD JI Aviat. Space Environ. Med. PD JUN PY 2009 VL 80 IS 6 BP 556 EP 560 DI 10.3357/ASEM.2363.2009 PG 5 WC Public, Environmental & Occupational Health; Medicine, General & Internal; Sport Sciences SC Public, Environmental & Occupational Health; General & Internal Medicine; Sport Sciences GA 454LM UT WOS:000266683400009 PM 19522367 ER PT J AU Zwart, SR Wolf, M Rogers, A Rodgers, S Gillman, PL Hitchcox, K Ericson, KL Smith, SM AF Zwart, Sara R. Wolf, Megan Rogers, Ann Rodgers, Shanna Gillman, Patti L. Hitchcox, Kristen Ericson, Karen L. Smith, Scott M. TI Stability of analytes related to clinical chemistry and bone metabolism in blood specimens after delayed processing SO CLINICAL BIOCHEMISTRY LA English DT Article; Proceedings Paper CT Experimental Biology 2008 Annual Meeting CY APR 05-09, 2008 CL San Diego, CA SP Amer Soc Pharmacol & Expt Therapeut, Amer Soc Investigat Pathol, Amer Soc Nutr, Amer Soc Biochem & Mol Biol, Amer Assoc Immunologists, Amer Assoc Anatomists, Amer Physiol Soc DE Centrifugation; Clinical chemistry; Nutrition assessment; Nutritional status; Space flight ID WHOLE-BLOOD; PLASMA; SERUM; TEMPERATURE; STORAGE AB Objectives: We investigated the stability of 36 analytes related to clinical chemistry in a controlled storage study. Design and methods: Blood was collected from 11 subjects and was maintained for 45 min, 2.5 h, 5 h, or 24 h after phlebotomy before centrifugation. Results: Statistically significant changes were observed only for parathyroid hormone, osteocalcin, zinc, pyridoxal 5'-phosphate, and homocysteine. Conclusions: These studies indicate that many analytes in clinical chemistry are stable for 24 h before centrifugation. (c) 2009 The Canadian Society of Clinical Chemists. Published by Elsevier Inc. All rights reserved. C1 [Zwart, Sara R.] Univ Space Res Assoc, Houston, TX USA. [Wolf, Megan] Oregon State Univ, Corvallis, OR 97331 USA. [Rogers, Ann; Rodgers, Shanna; Gillman, Patti L.] Enterprise Advisory Serv Inc, Houston, TX USA. [Hitchcox, Kristen] Colby Coll, Waterville, ME 04901 USA. [Ericson, Karen L.] Indiana Univ Purdue Univ, Ft Wayne, IN 46805 USA. [Smith, Scott M.] NASA, Human Adaptat & Countermeasures Div, Houston, TX 77058 USA. RP Zwart, SR (reprint author), NASA, Lyndon B Johnson Space Ctr, Attn Mail Code SK3,2 101 NASA Pkwy, Houston, TX 77058 USA. EM sara.zwart-1@nasa.gov NR 10 TC 10 Z9 10 U1 1 U2 3 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0009-9120 J9 CLIN BIOCHEM JI Clin. Biochem. PD JUN PY 2009 VL 42 IS 9 BP 907 EP 910 DI 10.1016/j.clinbiochem.2009.02.010 PG 4 WC Medical Laboratory Technology SC Medical Laboratory Technology GA 448XS UT WOS:000266295900026 PM 19250930 ER PT J AU Olson, SL Miller, FJ Jahangirian, S Wichman, IS AF Olson, S. L. Miller, F. J. Jahangirian, S. Wichman, I. S. TI Flame spread over thin fuels in actual and simulated microgravity conditions SO COMBUSTION AND FLAME LA English DT Article DE Flame spread; Microgravity; Thin fuel; Near-limit; Narrow channel; Flamelet ID FLOW AB Most previous research on flame spread over solid surfaces has involved flames in open areas. In this Study, the flame spreads in a narrow gap, as occurs in fires behind walls or inside electronic equipment. This geometry leads to interesting flame behaviors not typically seen in open flame spread, and also reproduces some of the conditions experienced by microgravity flames. Two sets of experiments are described, one involving flame spread in a Narrow Channel Apparatus (NCA) in normal gravity, and the others taking place in actual microgravity. Three primary variables are considered: flow velocity, oxygen concentration, and gap size (or effect of heat loss). When the oxidizer flow is reduced at either gravity level, the initially uniform flame front becomes corrugated and breaks into separate flamelets. This breakup behavior allows the flame to keep propagating below standard extinction limits by increasing the oxidizer transport to the flame, but has not been observed in other microgravity experiments due to the narrow samples employed. Breakup cannot be studied in typical (i.e., "open") normal gravity test facilities due to buoyancy-induced opposed flow velocities that are larger than the forced velocities in the flamelet regime. Flammability maps are constructed that delineate the uniform regime, the flamelet regime, and extinction limits for thin cellulose samples. Good agreement is found between flame and flamelet spread rate and flamelet size between the two facilities. Supporting calculations using FLUENT suggest that for small gaps buoyancy is suppressed and exerts a negligible influence on the flow pattern for inlet velocities >= 5 cm/s. The experiments show that in normal gravity the flamelets are a fire hazard since they can persist in small gaps where they are hard to detect. The results also indicate that the NCA quantitatively captures the essential features of the microgravity tests for thin fuels in opposed flow. Published by Elsevier Inc. on behalf of The Combustion Institute. C1 [Olson, S. L.] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. [Miller, F. J.] San Diego State Univ, Dept Mech Engn, San Diego, CA 92182 USA. [Jahangirian, S.; Wichman, I. S.] Michigan State Univ, E Lansing, MI 48824 USA. RP Olson, SL (reprint author), NASA, Glenn Res Ctr, Mail Stop 77-5,21000 Brookpk Rd, Cleveland, OH 44135 USA. EM Sandra.L.Olson@nasa.gov FU NASA Cooperative Agreement [NNC04AA50A, NCC31053] FX This work is supported by NASA Cooperative Agreement NNC04AA50A and NCC31053 with MSU. We thank the ATHINA engineering team, especially Jim Bruewer, and the Zero Gravity Research Facility personnel for their support of this work. Thanks also to Dr. Paul Ferkul for his help with some of the figures. NR 31 TC 20 Z9 25 U1 0 U2 12 PU ELSEVIER SCIENCE INC PI NEW YORK PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA SN 0010-2180 J9 COMBUST FLAME JI Combust. Flame PD JUN PY 2009 VL 156 IS 6 BP 1214 EP 1226 DI 10.1016/j.combustflame.2009.01.015 PG 13 WC Thermodynamics; Energy & Fuels; Engineering, Multidisciplinary; Engineering, Chemical; Engineering, Mechanical SC Thermodynamics; Energy & Fuels; Engineering GA 443EB UT WOS:000265891900007 ER PT J AU Choi, SR Kowalik, RW Alexander, DJ Bansal, NP AF Choi, Sung R. Kowalik, Robert W. Alexander, Donald J. Bansal, Narottam P. TI Elevated-temperature stress rupture in interlaminar shear of a Hi-Nic SiC/SiC ceramic matrix composite SO COMPOSITES SCIENCE AND TECHNOLOGY LA English DT Article DE Ceramic matrix composite; Mechanical properties; MI SiC/SiC; Interlaminar shear; Life prediction; Stress rupture ID CRACK-GROWTH; STRENGTH; INPLANE AB Assessments of stress rupture in a gas-turbine grade, melt-infiltrated Hi-Nicalon (TM) SiC continuous fiber-reinforced SiC ceramic matrix composite (CMC) were made in interlaminar shear at 1316 degrees C in air. The composite exhibited appreciable life limiting behavior with a life susceptibility parameter of n(s) = 22-24, estimated based on a proposed phenomenological life prediction model together with experimental data. The phenomenological life model was in good agreement in prediction between the stress rupture and the constant stress-rate data, validating its appropriateness in describing the life limiting phenomenon of the CIVIC coupons subjected to interlaminar shear. The results of this work also indicated that the governing mechanism(s) associated with failure in interlaminar shear would have remained almost unchanged, regardless of the type of loading configurations, either in stress rupture or in constant stress rate. Published by Elsevier Ltd. C1 [Choi, Sung R.; Kowalik, Robert W.; Alexander, Donald J.] Naval Air Syst Command, Patuxent River, MD 20670 USA. [Bansal, Narottam P.] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. RP Choi, SR (reprint author), Naval Air Syst Command, 48066 Shaw Rd, Patuxent River, MD 20670 USA. EM sung.choil@navy.mil FU NAVAIR; Office of Naval Research FX The authors (NAVAIR) acknowledge Dr. D. Shifler and the Office of Naval Research for the support of this work. Some mechanical testing was conducted at the NASA Glenn, Cleveland, Ohio. NR 24 TC 11 Z9 11 U1 0 U2 15 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 0266-3538 J9 COMPOS SCI TECHNOL JI Compos. Sci. Technol. PD JUN PY 2009 VL 69 IS 7-8 BP 890 EP 897 DI 10.1016/j.compscitech.2008.12.006 PG 8 WC Materials Science, Composites SC Materials Science GA 450DH UT WOS:000266380700003 ER PT J AU Zhang, Y Rohde, LH Wu, HL AF Zhang, Ye Rohde, Larry H. Wu, Honglu TI Involvement of Nucleotide Excision and Mismatch Repair Mechanisms in Double Strand Break Repair SO CURRENT GENOMICS LA English DT Review DE Ionizing radiation (IR); DNA damage; DSB repair; NER; MMR and cell cycle ID REPLICATION PROTEIN-A; INTERSTRAND CROSS-LINK; CELL-CYCLE CHECKPOINT; PIGMENTOSUM GROUP-A; SACCHAROMYCES-CEREVISIAE MSH2; GROUP-C GENE; DNA-DAMAGE; XERODERMA-PIGMENTOSUM; IONIZING-RADIATION; HOMOLOGOUS RECOMBINATION AB Living organisms are constantly threatened by environmental DNA-damaging agents, including UV and ionizing radiation (IR). Repair of various forms of DNA damage caused by IR is normally thought to follow lesion-specific repair pathways with distinct enzymatic machinery. DNA double strand break is one of the most serious kinds of damage induced by IR, which is repaired through double strand break (DSB) repair mechanisms, including homologous recombination (HR) and non-homologous end joining (NHEJ). However, recent studies have presented increasing evidence that various DNA repair pathways are not separated, but well interlinked. It has been suggested that non-DSB repair mechanisms, such as Nucleotide Excision Repair (NER), Mismatch Repair (MMR) and cell cycle regulation, are highly involved in DSB repairs. These findings revealed previously unrecognized roles of various non-DSB repair genes and indicated that a successful DSB repair requires both DSB repair mechanisms and non-DSB repair systems. One of our recent studies found that suppressed expression of non-DSB repair genes, such as XPA, RPA and MLH1, influenced the yield of IR-induced micronuclei formation and/or chromosome aberrations, suggesting that these genes are highly involved in DSB repair and DSB-related cell cycle arrest, which reveals new roles for these gene products in the DNA repair network. In this review, we summarize current progress on the function of non-DSB repair-related proteins, especially those that participate in NER and MMR pathways, and their influence on DSB repair. In addition, we present our developing view that the DSB repair mechanisms are more complex and are regulated by not only the well known HR/NHEJ pathways, but also a systematically coordinated cellular network. C1 [Zhang, Ye] NASA, Johnson Space Ctr, Human Adaptat & Countermeasures Div, Houston, TX 77058 USA. [Zhang, Ye; Rohde, Larry H.] Univ Houston Clear Lake City, Houston, TX 77058 USA. RP Zhang, Y (reprint author), NASA, Johnson Space Ctr, Human Adaptat & Countermeasures Div, Mail Code SK,2101 NASA Pkwy, Houston, TX 77058 USA. EM Ye.Zhang-1@nasa.gov NR 125 TC 40 Z9 40 U1 1 U2 9 PU BENTHAM SCIENCE PUBL LTD PI SHARJAH PA EXECUTIVE STE Y26, PO BOX 7917, SAIF ZONE, 1200 BR SHARJAH, U ARAB EMIRATES SN 1389-2029 J9 CURR GENOMICS JI Curr. Genomics PD JUN PY 2009 VL 10 IS 4 BP 250 EP 258 PG 9 WC Biochemistry & Molecular Biology; Genetics & Heredity SC Biochemistry & Molecular Biology; Genetics & Heredity GA 452UC UT WOS:000266565700005 PM 19949546 ER PT J AU Qu, TD Song, YT Yamagata, T AF Qu, Tangdong Song, Y. Tony Yamagata, Toshio TI An introduction to the South China Sea throughflow: Its dynamics, variability, and application for climate SO DYNAMICS OF ATMOSPHERES AND OCEANS LA English DT Review DE South China Sea throughflow; Western boundary current; Indonesian throughflow; Asian climate ID NORTH EQUATORIAL CURRENT; WESTERN BOUNDARY CURRENTS; DEPTH-INTEGRATED FLOW; INDONESIAN THROUGHFLOW; INDIAN-OCEAN; SURFACE TEMPERATURE; MARITIME CONTINENT; INTERANNUAL VARIABILITY; CURRENT BIFURCATION; KUROSHIO INTRUSION AB The South China Sea throughflow (SCSTF) involves the inflow through the Luzon strait and the outflow through the Karimata, Mindoro, and Taiwan straits. Recent studies have suggested that the SCSTF act as a heat and freshwater conveyor, playing a potentially important role in regulating the sea surface temperature pattern in the South China Sea and its adjoining tropical Indian and Pacific Oceans. In this introductory paper, we attempt to convey the progress that has recently been made in understanding the SCSTF. We first provide an overview of existing observations, theories, and simulations of the SCSTF. Then, we discuss its interaction with the Pacific western boundary current and Indonesian throughflow. Finally, we summarize issues and questions that remain to be addressed, with special reference to the SCSTF's dynamics, variability, and implication for climate. (c) 2008 Elsevier B.V. All rights reserved. C1 [Qu, Tangdong] Univ Hawaii Manoa, SOEST, Int Pacific Res Ctr, Honolulu, HI 96822 USA. [Song, Y. Tony] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Yamagata, Toshio] Univ Tokyo, Dept Earth & Planetary Sci, Tokyo, Japan. RP Qu, TD (reprint author), Univ Hawaii Manoa, SOEST, Int Pacific Res Ctr, 1680 East West Rd, Honolulu, HI 96822 USA. EM tangdong@hawaii.edu RI Yamagata, Toshio/A-1807-2009 FU U.S. National Science Foundation [OCE-0623533]; Japan Society for Promotion of Science [17204040]; Japan Agency for Marine-Earth Science and Technology; National Ocean and Atmosphere Administration; National Aeronautics and Space Administration; School of Ocean and Earth Science and Technology [7471]; IPRC [IPRC-525] FX This research was supported by the U.S. National Science Foundation through grant OCE-0623533 and by the Japan Society for Promotion of Science through Grant-in-Aid for Scientific Research (A) 17204040. Support for TQ was also from Japan Agency for Marine-Earth Science and Technology, from the National Ocean and Atmosphere Administration, and from the National Aeronautics and Space Administration through their sponsorship of the International Pacific Research Center (IPRC). The authors are grateful to A.M. Moore for his strong support for the special issue. School of Ocean and Earth Science and Technology contribution number 7471, and IPRC contribution number IPRC-525. NR 90 TC 64 Z9 73 U1 6 U2 44 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0377-0265 J9 DYNAM ATMOS OCEANS JI Dyn. Atmos. Oceans PD JUN PY 2009 VL 47 IS 1-3 SI SI BP 3 EP 14 DI 10.1016/j.dynatmoce.2008.05.001 PG 12 WC Geochemistry & Geophysics; Meteorology & Atmospheric Sciences; Oceanography SC Geochemistry & Geophysics; Meteorology & Atmospheric Sciences; Oceanography GA 433AD UT WOS:000265174800002 ER PT J AU Gudipati, MS AF Gudipati, Murthy S. TI Editorial for Earth, Moon, and Planets SO EARTH MOON AND PLANETS LA English DT Editorial Material C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Gudipati, MS (reprint author), CALTECH, Jet Prop Lab, M-S 183-301,4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM Murthy.Gudipati@jpl.nasa.gov RI Gudipati, Murthy/F-7575-2011 NR 0 TC 0 Z9 0 U1 1 U2 6 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0167-9295 J9 EARTH MOON PLANETS JI Earth Moon Planets PD JUN PY 2009 VL 105 IS 1 BP 1 EP 2 DI 10.1007/s11038-009-9332-9 PG 2 WC Astronomy & Astrophysics; Geosciences, Multidisciplinary SC Astronomy & Astrophysics; Geology GA 474PT UT WOS:000268297100001 ER PT J AU Molotch, NP Brooks, PD Burns, SP Litvak, M Monson, RK McConnell, JR Musselman, K AF Molotch, Noah P. Brooks, Pald D. Burns, Sean P. Litvak, Marcy Monson, Russell K. McConnell, Joseph R. Musselman, Keith TI Ecohydrological controls on snowmelt partitioning in mixed-conifer sub-alpine forests SO ECOHYDROLOGY LA English DT Article DE snowmelt infiltration; evapotranspiration; snow-vegetation interactions; vegetation change ID WESTERN NORTH-AMERICA; HIGH-ELEVATION; ENERGY-BALANCE; VALLES CALDERA; BOREAL FOREST; WATER YIELD; NEW-MEXICO; COVER; CLIMATE; MODEL AB We used co-located observations of snow depth, soil temperature, and moisture and energy fluxes to monitor variability in snowmelt infiltration and vegetation water use at mixed-conifer sub-alpine forest sites in the Valles Caldera, New Mexico (3020 m) and on Niwot Ridge, Colorado (3050 in). At both sites, vegetation structure largely controlled the distribution of snow accumulation with 29% greater accumulation in open versus under-canopy locations. Snow ablation rates were diminished by 39% in under-canopy locations, indicating increases in vegetation density act to extend the duration of the snowmelt season. Similarly, differences in climate altered snow-season duration, snowmelt infiltration and evapotranspiration. Commencement of the,rowing season,vas coincident with melt-water input to the soil and lagged behind springtime increases in air temperature by 12 days oil average, ranging from 2 to 33 days Under warmer and colder conditions, respectively. Similarly, the timing of peak Soil moisture was highly variable, lagging behind springtime increases in air temperature by 42 and 31 days oil average at the Colorado and New Mexico sites, respectively. Latent heat flux and associated evaporative loss to the atmosphere was 28% greater For the year with earlier onset of snowmelt infiltration. Given the large and variable fraction of precipitation that was Partitioned into water vapour loss, the combined effects of changes in vegetation structure, climate and associated changes to the timing and magnitude of snowmelt may have large effects oil the partitioning of snowmelt into evapotranspiration, surface runoff and ground water recharge. Copyright (C) 2009 John Wiley & Sons, Ltd. C1 [Molotch, Noah P.; Musselman, Keith] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Molotch, Noah P.; Musselman, Keith] Univ Calif Los Angeles, Dept Civil & Environm Engn, Los Angeles, CA 90095 USA. [Brooks, Pald D.] Univ Arizona, Dept Hydrol & Water Resources, Tucson, AZ 85721 USA. [Burns, Sean P.] Natl Ctr Atmospher Res, Boulder, CO 80307 USA. [Litvak, Marcy] Univ New Mexico, Dept Biol, Albuquerque, NM 87131 USA. [Burns, Sean P.; Monson, Russell K.] Univ Colorado, Dept Ecol & Evolut Biol, Boulder, CO 80309 USA. [Burns, Sean P.; Monson, Russell K.] Univ Colorado, Cooperat Inst Res Environm Sci, Boulder, CO 80309 USA. [McConnell, Joseph R.] Desert Res Inst, Reno, NV 89512 USA. RP Molotch, NP (reprint author), CALTECH, Jet Prop Lab, M-S 300-233,4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM molotch@seas.ucla.edu RI Molotch, Noah/C-8576-2009; Burns, Sean/A-9352-2008; Breshears, David/B-9318-2009 OI Burns, Sean/0000-0002-6258-1838; Breshears, David/0000-0001-6601-0058 FU National Science Foundation, Hydrologic Sciences Program; [NSFEAR0711600] FX This research was supported by the National Science Foundation, Science and Technology Center for the Sustainability of semi-Arid Hydrology and Riparian Areas (SAHRA). Additional support was provided by a research fellowship at the Cooperative Institute for Research in Environmental Sciences, University of Colorado, Boulder, by the National Science Foundation, Hydrologic Sciences Program (NSFEAR0711600) and by the NOAA Office of Hydrologic Development. The work at Niwot Ridge was funded in part by a grant from the Western Section of the National Institute for Climate Change Research (NICCR-MPC35TX-A2) administered by Northern Arizona University and funded by the US Department of Energy (BER Program). R. Bales, M. Williams and J. Beauregard are acknowledged for technical support. Field teams are acknowledged with thanks. Bob Parmenter and the Valles Caldera Trust are acknowledged for supporting research activities in the Valles Caldera NR 55 TC 65 Z9 65 U1 3 U2 51 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1936-0584 EI 1936-0592 J9 ECOHYDROLOGY JI Ecohydrology PD JUN PY 2009 VL 2 IS 2 BP 129 EP 142 DI 10.1002/eco.48 PG 14 WC Ecology; Environmental Sciences; Water Resources SC Environmental Sciences & Ecology; Water Resources GA 470IK UT WOS:000267968200002 ER PT J AU Morisette, JT Richardson, AD Knapp, AK Fisher, JI Graham, EA Abatzoglou, J Wilson, BE Breshears, DD Henebry, GM Hanes, JM Liang, L AF Morisette, Jeffrey T. Richardson, Andrew D. Knapp, Alan K. Fisher, Jeremy I. Graham, Eric A. Abatzoglou, John Wilson, Bruce E. Breshears, David D. Henebry, Geoffrey M. Hanes, Jonathan M. Liang, Liang TI Tracking the rhythm of the seasons in the face of global change: phenological research in the 21st century SO FRONTIERS IN ECOLOGY AND THE ENVIRONMENT LA English DT Review ID LAND-SURFACE PHENOLOGY; DIGITAL CAMERA; VEGETATION STRUCTURE; CLIMATE; ECOSYSTEMS; TEMPERATURE; MODELS; PREDICTION; PROGRAM; IMAGES AB Phenology is the study of recurring life-cycle events, classic examples being the flowering of plants and animal migration. Phenological responses are increasingly relevant for addressing applied environmental issues. Yet, challenges remain with respect to spanning scales of observation, integrating observations across taxa, and modeling phenological sequences to enable ecological forecasts in light of future climate change. Recent advances that are helping to address these questions include refined landscape-scale phenology estimates from satellite data, advanced, instrument-based approaches for field measurements, and new cyberinfrastructure for archiving and distribution of products. These breakthroughs are improving our understanding in diverse areas, including modeling land-surface exchange, evaluating climate-phenology relationships, and making land-management decisions. C1 [Morisette, Jeffrey T.] NASA, Goddard Space Flight Ctr, Greenbelt, MD USA. [Richardson, Andrew D.] Univ New Hampshire, Complex Syst Res Ctr, Durham, NH 03824 USA. [Knapp, Alan K.] Colorado State Univ, Dept Biol, Ft Collins, CO 80523 USA. [Knapp, Alan K.] Colorado State Univ, Grad Degree Program Ecol, Ft Collins, CO 80523 USA. [Fisher, Jeremy I.] Synapse Energy Econ Inc, Cambridge, MA USA. [Graham, Eric A.] Univ Calif Los Angeles, Ctr Embedded Networked Sensing, Los Angeles, CA USA. [Abatzoglou, John] Univ Nevada, Desert Res Inst, Western Reg Climate Ctr, Div Atmospher Sci, Reno, NV 89506 USA. [Wilson, Bruce E.] Oak Ridge Natl Lab, Div Environm Sci, Oak Ridge, TN 37831 USA. [Breshears, David D.] Univ Arizona, Sch Nat Resources, Inst Study Planet Earth, Tucson, AZ USA. [Breshears, David D.] Univ Arizona, Dept Ecol & Evolut Biol, Tucson, AZ 85721 USA. [Henebry, Geoffrey M.] S Dakota State Univ, Geog Informat Sci Ctr Excellence, Brookings, SD 57007 USA. [Hanes, Jonathan M.; Liang, Liang] Univ Wisconsin Milwaukee, Dept Geog, Milwaukee, WI USA. RP Morisette, JT (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD USA. EM mori-settej@usgs.gov RI Breshears, David/B-9318-2009; Richardson, Andrew/F-5691-2011; Abatzoglou, John/C-7635-2012; Knapp, Alan/A-2931-2008; OI Breshears, David/0000-0001-6601-0058; Richardson, Andrew/0000-0002-0148-6714; Abatzoglou, John/0000-0001-7599-9750; Wilson, Bruce/0000-0002-1421-1728; Graham, Eric/0000-0002-7495-4056; Henebry, Geoffrey/0000-0002-8999-2709 FU National Science Foundation Research [0639794] FX The authors thank JL Betancourt and MD Schwartz for their leadership in developing the USA National Phenology Network. It was through the August 2007 annual meeting of the USA-NPN Research Coordination Network (supported by National Science Foundation Research grant # 0639794) that the authors came together to develop this paper. The authors thank JF Weltzin for his leadership at that meeting and J Gross, who led the session calling for a phenology review paper. Please see WebPanel 1 for author contributions. NR 51 TC 182 Z9 190 U1 11 U2 132 PU ECOLOGICAL SOC AMER PI WASHINGTON PA 1990 M STREET NW, STE 700, WASHINGTON, DC 20036 USA SN 1540-9295 J9 FRONT ECOL ENVIRON JI Front. Ecol. Environ. PD JUN PY 2009 VL 7 IS 5 BP 253 EP 260 DI 10.1890/070217 PG 8 WC Ecology; Environmental Sciences SC Environmental Sciences & Ecology GA 456SV UT WOS:000266869700021 ER PT J AU Brady, RA Peters, BT Bloomberg, JJ AF Brady, Rachel A. Peters, Brian T. Bloomberg, Jacob J. TI Strategies of healthy adults walking on a laterally oscillating treadmill SO GAIT & POSTURE LA English DT Article DE Human locomotion; Unstable surface; Sensory weighting; Adaptation; Stability ID OBSTACLE AVOIDANCE; VIRTUAL-REALITY; SPACE-FLIGHT; VISUAL CONTROL; OPTIC FLOW; TASK; ADAPTATION; LOCOMOTION; SURFACE; ENVIRONMENT AB We mounted a treadmill on top of a six degree-of-freedom motion base platform to investigate locomotor responses produced by healthy adults introduced to a dynamic walking surface. The experiment examined self-selected strategies employed by participants when exposed to continuous, sinusoidal lateral motion of the support surface while walking. Torso translation and step width were used to classify responses used to stabilize gait in this novel, dynamic environment. Two response categories emerged. Participants tended to either fix themselves in space (FIS), allowing the treadbelt to move laterally beneath them, or fix themselves to the base (FTB), moving laterally as the motion base oscillated. The degree of fixation in both extremes varied across participants. This finding Suggests that normal adults have innate and varied preferences for optimizing gait stability, some depending more heavily on vision (FIS group) and others on proprioception (FTB group). (C) 2009 Elsevier B.V. All rights reserved. C1 [Brady, Rachel A.; Peters, Brian T.] Wyle Integrated Sci & Engn Grp, Houston, TX 77058 USA. [Bloomberg, Jacob J.] NASA, Lyndon B Johnson Space Ctr, Neurosci Labs, Houston, TX 77058 USA. RP Brady, RA (reprint author), Wyle Integrated Sci & Engn Grp, 1290 Hercules Dr, Houston, TX 77058 USA. EM rachel.brady-1@nasa.gov FU National Space Biomedical Research Institute through NASA NCC [9-58] FX This work was Supported by the National Space Biomedical Research Institute through NASA NCC 9-58. NR 30 TC 12 Z9 12 U1 2 U2 2 PU ELSEVIER IRELAND LTD PI CLARE PA ELSEVIER HOUSE, BROOKVALE PLAZA, EAST PARK SHANNON, CO, CLARE, 00000, IRELAND SN 0966-6362 J9 GAIT POSTURE JI Gait Posture PD JUN PY 2009 VL 29 IS 4 BP 645 EP 649 DI 10.1016/j.gaitpost.2009.01.010 PG 5 WC Neurosciences; Orthopedics; Sport Sciences SC Neurosciences & Neurology; Orthopedics; Sport Sciences GA 437GX UT WOS:000265476000023 PM 19233653 ER PT J AU Debaille, V Tronnes, RG Brandon, AD Waight, TE Graham, DW Lee, CTA AF Debaille, Vinciane Tronnes, Reidar G. Brandon, Alan D. Waight, Tod E. Graham, David W. Lee, Cin-Ty A. TI Primitive off-rift basalts from Iceland and Jan Mayen: Os-isotopic evidence for a mantle source containing enriched subcontinental lithosphere SO GEOCHIMICA ET COSMOCHIMICA ACTA LA English DT Review ID OCEAN ISLAND BASALTS; MID-ATLANTIC RIDGE; SNAEFELL VOLCANIC CENTER; NORWEGIAN-GREENLAND SEA; HIGH HE-3/HE-4 RATIOS; V-SHAPED RIDGES; ABYSSAL PERIDOTITES; SR ISOTOPE; TRACE-ELEMENT; EARTHS MANTLE AB New measurements of Os, He, Sr and Nd isotopes, along with major and trace elements, are presented for basalts from the three volcanic flank zones in Iceland and from Jan Mayen Island. The Os-187/Os-188 ratios in lavas with <30 ppt Os (n = 4) are elevated compared to ratios in coexisting olivine and appear to be contaminated at a shallow level. The Os-187/Os-188 ratios in the remaining lavas with >30 ppt Os (n = 17) range between 0.12117 and 0.13324. These values are surprisingly low for oceanic island basalts and include some samples that are less than putative present-day primitive upper mantle (PUM with Os-187/Os-188 of 0.1296). These low Os-187/Os-188 preclude significant shallow-level contamination from oceanic crust. The Os-187/Os-188 ratios for Jan Mayen lavas are less than PUM, severely limiting the presence of any continental crust in their mantle source. A positive correlation between Nd-143/Nd-144 and Os-187/Os-188 ratios in Iceland and Jan Mayen lavas likely reflects the presence in their source of ancient subcontinental lithosphere that has undergone incompatible trace element enrichment that did not affect the Re-Os system. In addition, the Jan Mayen lava isotopic signature cannot be explained solely by the presence of subcontinental lithospheric mantle, and the influence of another geochemical component, such as a mantle plume appears required. Combined Sr-87/Sr-86, Nd-143/Nd-144, He-3/He-4 and Os-187/Os-188 data indicate a genetic relationship between Jan Mayen Island and the Iceland mantle plume. Material from the Iceland mantle plume likely migrates at depth until it reaches the tensional setting of the Jan Mayen Fracture Zone, where it undergoes low-degree partial melting. At a first-order, isotopic co-variations can be interpreted as broadly binary Mixing Curves between two primary end-members. One end-member, characterized in particular by its unradiogenic Os-187/Os-188 and Nd-143/Nd-144, low He-3/He-4 and high Sr-87/Sr-86, is represented by subcontinental lithospheric mantle stranded and disseminated in the upper mantle during the opening of the Atlantic Ocean. The second end-member corresponds to a hybrid mixture between the depleted-MORB mantle and the enriched Iceland mantle plume, itself resulting from mixing between recycled oceanic crust and depleted lower mantle. This hybrid accounts for the high He-3/He-4 (similar to 28 Ra), high Nd-143/Nd-144 (similar to 0.5132), high Os-187/Os-188 (similar to 0.14) and low Sr-87/Sr-86 (similar to 0.7026) composition observed in Iceland. Two different models may account for these observed mixing relationships mantle and allows refractory sub-lithospheric fragments to melt because of excess heat derived from the deep plume material. A second model that may better account for the Pb isotopic variations observed, uses the same components but where the depleted-MORB mantle is already polluted by subcontinental lithospheric mantle material before mixing with the Iceland mantle plume. Both cases likely occur. Though only three principal components are required to explain the isotopic variations of the Iceland-Jan Mayen system, the different possible mixing relationships may be accounted for by potentially a greater number of en-members. (C) 2009 Elsevier Ltd. All rights reserved. C1 [Debaille, Vinciane] Univ Libre Brussels, Dept Sci Terre & Environm, B-1050 Brussels, Belgium. [Debaille, Vinciane] Lunar & Planetary Inst, Houston, TX 77058 USA. [Tronnes, Reidar G.] Univ Iceland, Inst Earth Sci, Nord Volcanol Ctr, Reykjavik, Iceland. [Tronnes, Reidar G.] Univ Oslo, Nat Hist Museum, N-0318 Oslo, Norway. [Brandon, Alan D.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. [Waight, Tod E.] Univ Copenhagen, Inst Geog & Geol, DK-1350 Copenhagen K, Denmark. [Graham, David W.] Oregon State Univ, Coll Ocean & Atmospher Sci, Corvallis, OR 97331 USA. [Lee, Cin-Ty A.] Rice Univ, Dept Earth Sci, Houston, TX 77251 USA. RP Debaille, V (reprint author), Univ Libre Brussels, Dept Sci Terre & Environm, CP160102,50 Av FD Roosevelt, B-1050 Brussels, Belgium. EM vinciane.debaille@ulb.ac.be RI Lee, Cin-Ty/A-5469-2008; Waight, Tod/A-8262-2010; OI Waight, Tod/0000-0003-2601-1202; Graham, David/0000-0002-7411-1905 NR 163 TC 28 Z9 28 U1 2 U2 33 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0016-7037 J9 GEOCHIM COSMOCHIM AC JI Geochim. Cosmochim. Acta PD JUN 1 PY 2009 VL 73 IS 11 BP 3423 EP 3449 DI 10.1016/j.gca.2009.03.002 PG 27 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 445OI UT WOS:000266059700021 ER PT J AU Marion, GM Crowley, JK Thomson, BJ Kargel, JS Bridges, NT Hook, SJ Baldridge, A Brown, AJ da Luz, BR de Souza, CR AF Marion, G. M. Crowley, J. K. Thomson, B. J. Kargel, J. S. Bridges, N. T. Hook, S. J. Baldridge, A. Brown, A. J. da Luz, B. Ribeiro de Souza Filho, C. R. TI Modeling aluminum-silicon chemistries and application to Australian acidic playa lakes as analogues for Mars SO GEOCHIMICA ET COSMOCHIMICA ACTA LA English DT Article ID RIO-TINTO BASIN; MERIDIANI-PLANUM; OMEGA/MARS EXPRESS; LOW-TEMPERATURES; MOSSBAUER SPECTROMETER; THERMODYNAMIC MODEL; TERRESTRIAL ANALOGS; WESTERN-AUSTRALIA; BURNS FORMATION; IRON CHEMISTRY AB Recent Mars missions have stimulated considerable thinking about the surficial geochemical evolution of Mars. Among the major relevant findings are the presence in Meridiani Planum sediments of the mineral jarosite (a ferric sulfate salt) and related minerals that require formation from all acid-salt brine and oxidizing environment. Similar mineralogies have been observed in acidic saline lake sediments in Western Australia (WA), and these lakes have been proposed as analogues for acidic sedimentary environments oil Mars. The prior version of the equilibrium chemical thermodynamic FREZCHEM model lacked Al and Si chemistries that are needed to appropriately model acidic aqueous geochemistries oil Earth and Mars. The objectives of this work were to (1) add Al and Si chemistries to the FREZCHEM model, (2) extend these chemistries to low temperatures (<0 degrees C), if possible, and (3) use the reformulated model to investigate parallels in the mineral precipitation behavior of acidic Australian lakes and hypothetical Martian brines. FREZCHEM is an equilibrium chemical thermodynamic model parameterized for concentrated electrolyte solutions using the Pitzer approach for the temperature range from <-70 to 25 degrees C and the pressure range from I to 1000 bars. Aluminum chloride and sulfate mineral parameterizations were based oil experimental data. Aluminum hydroxide and silicon mineral parameterizations were based oil Gibbs free energy and enthalpy data. New aluminum and silicon parameterizations added 12 new aluminum/silicon minerals to this Na-K-Mg-Ca-Fe(II)-Fe(III)-Al-H-Cl-Br-SO4-NO3-OH-HCO3-CO3-CO2-O-2-CH4-Si-H2O system that now contain 95 solid phases. There were similarities, differences, and uncertain ties between Australian acidic, saline playa lakes and waters that likely led to the Burns formation salt accumulations oil Mars. Both systems are similar in that they are dominated by ( 1) acidic, saline ground waters and sediments, (2) Ca apointing to the dominant influence of ground water chemistry, vertical such lateral variations are much less pronounced.nd/or Mg sulfates, and (3) iron precipitates Such as jarosite and hematite. Differences include: (1) the dominance of NaCl in many WA lakes, versus the dominance of Fe-Mg-Ca-SO4 in Meridiani Planum, (2) excessively low K+ concentrations in Meridiani Planum due to jarosite precipitation, (3) higher acid production in the presence of high iron concentrations in Meridiani Planum, and probably lower rates of acid neutralization and hence, higher acidities oil Mars owing to colder temperatures, and (4) lateral salt patterns in WA lakes. The WA playa lakes display significant lateral variations in mineralogy and water chemistry over short distances, reflecting the interaction of acid ground waters with neutral to alkaline lake waters derived from ponded surface runoff. Meridiani Planum observations indicate that such lateral variations are much less pronounced, pointing to the dominant influence of ground water chemistry, vertical ground water movements, and aeolian processes on the Martian surface mineralogy. (C) 2009 Elsevier Ltd. All rights reserved. C1 [Marion, G. M.] Desert Res Inst, Reno, NV 89512 USA. [Crowley, J. K.; da Luz, B. Ribeiro] US Geol Survey, Reston, VA 20192 USA. [Thomson, B. J.] Johns Hopkins Appl Phys Lab, Laurel, MD 20723 USA. [Kargel, J. S.] Univ Arizona, Tucson, AZ 85721 USA. [Bridges, N. T.; Hook, S. J.; Baldridge, A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Brown, A. J.] NASA, Ames Res Ctr, Mountain View, CA 94043 USA. [de Souza Filho, C. R.] Univ Estadual Campinas, Campinas, SP, Brazil. RP Marion, GM (reprint author), Desert Res Inst, 2215 Raggio Parkway, Reno, NV 89512 USA. EM giles.marion@dri.edu RI Bridges, Nathan/D-6341-2016; OI Thomson, Bradley/0000-0001-8635-8932 NR 84 TC 17 Z9 17 U1 2 U2 24 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0016-7037 EI 1872-9533 J9 GEOCHIM COSMOCHIM AC JI Geochim. Cosmochim. Acta PD JUN 1 PY 2009 VL 73 IS 11 BP 3493 EP 3511 DI 10.1016/j.gca.2009.03.013 PG 19 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 445OI UT WOS:000266059700024 ER PT J AU Adams, PJ Pandis, SN Dawson, JP Racherla, PN AF Adams, P. J. Pandis, S. N. Dawson, J. P. Racherla, P. N. TI Air quality in a changing climate SO GEOCHIMICA ET COSMOCHIMICA ACTA LA English DT Meeting Abstract CT 19th Annual VM Goldschmidt Conference CY JUN 21, 2009 CL Davos, SWITZERLAND C1 [Adams, P. J.] Carnegie Mellon Univ, Ctr Atmospher Particle Studies, Pittsburgh, PA 15213 USA. [Pandis, S. N.] Univ Patras, Dept Chem Engn, GR-26110 Patras, Greece. [Dawson, J. P.] US EPA, Washington, DC 20460 USA. [Racherla, P. N.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA. EM petera@andrew.cmu.edu RI Pandis, Spyros/D-3680-2013; Adams, Peter/D-7134-2013 OI Adams, Peter/0000-0003-0041-058X NR 0 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 0016-7037 J9 GEOCHIM COSMOCHIM AC JI Geochim. Cosmochim. Acta PD JUN PY 2009 VL 73 IS 13 BP A9 EP A9 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 460YS UT WOS:000267229900031 ER PT J AU Alperin, MJ Hoehler, TM AF Alperin, M. J. Hoehler, T. M. TI Bioenergetics in archaea/sulfate-reducing bacteria aggregates SO GEOCHIMICA ET COSMOCHIMICA ACTA LA English DT Meeting Abstract CT 19th Annual VM Goldschmidt Conference CY JUN 21, 2009 CL Davos, SWITZERLAND C1 [Alperin, M. J.] Univ N Carolina, Dept Marine Sci, Chapel Hill, NC 27599 USA. [Hoehler, T. M.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. EM alperin@email.unc.edu; tori.m.hoehler@nasa.gov NR 0 TC 0 Z9 0 U1 2 U2 6 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0016-7037 J9 GEOCHIM COSMOCHIM AC JI Geochim. Cosmochim. Acta PD JUN PY 2009 VL 73 IS 13 BP A32 EP A32 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 460YS UT WOS:000267229900076 ER PT J AU Beard, BL Handler, R Johnson, CM Scherer, M AF Beard, Brian L. Handler, Robert Johnson, Clark M. Scherer, Michelle TI Experimental determination of the Fe isotope fractionation between Fe(II) and goethite SO GEOCHIMICA ET COSMOCHIMICA ACTA LA English DT Meeting Abstract CT 19th Annual VM Goldschmidt Conference CY JUN 21, 2009 CL Davos, SWITZERLAND ID MOSSBAUER-SPECTROSCOPY; GEOCHEMISTRY C1 [Beard, Brian L.; Johnson, Clark M.] Univ Wisconsin, Madison, WI 53706 USA. [Beard, Brian L.; Johnson, Clark M.] NASA, Astrobiol Inst, Washington, DC USA. [Handler, Robert; Scherer, Michelle] Univ Iowa, Iowa City, IA 52242 USA. EM beardb@geology.wisc.edu NR 3 TC 3 Z9 3 U1 0 U2 1 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0016-7037 J9 GEOCHIM COSMOCHIM AC JI Geochim. Cosmochim. Acta PD JUN PY 2009 VL 73 IS 13 BP A99 EP A99 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 460YS UT WOS:000267229900210 ER PT J AU Bennett, V Brandon, A Hiess, J Nutman, A Black, L AF Bennett, V. Brandon, A. Hiess, J. Nutman, A. Black, L. TI Limited Hadean continents from combined Nd142-143-Hf-176 isotopic compositions of Eoarchean rocks SO GEOCHIMICA ET COSMOCHIMICA ACTA LA English DT Meeting Abstract CT 19th Annual VM Goldschmidt Conference CY JUN 21, 2009 CL Davos, SWITZERLAND C1 [Bennett, V.; Hiess, J.] Australian Natl Univ, Res Sch Earth Sci, Canberra, ACT 0200, Australia. [Brandon, A.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. [Nutman, A.] Chinese Acad Geol Sci, Beijing, Peoples R China. [Black, L.] Geosci Australia, Canberra, ACT, Australia. EM vickie.bennett@anu.edu.au NR 2 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 0016-7037 J9 GEOCHIM COSMOCHIM AC JI Geochim. Cosmochim. Acta PD JUN PY 2009 VL 73 IS 13 SU S BP A110 EP A110 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 460YS UT WOS:000267229900232 ER PT J AU Brown, I Thomas-Keprta, K Sarkisova, S Clarke, W Fischer, C Luttge, A Arvidson, R Shen, G Bryant, D Galindo, C Garrison, D McKay, DS AF Brown, I. Thomas-Keprta, K. Sarkisova, S. Clarke, W. Fischer, C. Luttge, A. Arvidson, R. Shen, G. Bryant, D. Galindo, C. Garrison, D. McKay, D. S. TI Cycling of Fe by siderophilic cyanobacteria: Implications for an early biosphere SO GEOCHIMICA ET COSMOCHIMICA ACTA LA English DT Meeting Abstract CT 19th Annual VM Goldschmidt Conference CY JUN 21, 2009 CL Davos, SWITZERLAND C1 [Brown, I.; Thomas-Keprta, K.; Sarkisova, S.; Clarke, W.; Galindo, C.; Garrison, D.; McKay, D. S.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. [Fischer, C.; Luttge, A.; Arvidson, R.] Rice Univ, Dpt Earth Sci, Hoston, TX USA. [Shen, G.; Bryant, D.] Penn State Univ, Dpt Biochem, University Pk, PA 16802 USA. EM igor.i.brown@nasa.gov RI Luttge, Andreas/A-2560-2011 OI Luttge, Andreas/0000-0002-5878-4026 NR 0 TC 0 Z9 0 U1 0 U2 0 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0016-7037 J9 GEOCHIM COSMOCHIM AC JI Geochim. Cosmochim. Acta PD JUN PY 2009 VL 73 IS 13 BP A163 EP A163 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 460YS UT WOS:000267229900339 ER PT J AU Chin, M Yu, HB Kahn, R Remer, L Diehl, T Prados, A Leptoukh, G AF Chin, Mian Yu, Hongbin Kahn, Ralph Remer, Lorraine Diehl, Thomas Prados, Ana Leptoukh, Gregory TI Possibilities and challenges in using satellite aerosol data for surface air quality studies SO GEOCHIMICA ET COSMOCHIMICA ACTA LA English DT Meeting Abstract CT 19th Annual VM Goldschmidt Conference CY JUN 21, 2009 CL Davos, SWITZERLAND C1 [Chin, Mian; Yu, Hongbin; Kahn, Ralph; Remer, Lorraine; Diehl, Thomas; Prados, Ana; Leptoukh, Gregory] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Yu, Hongbin; Diehl, Thomas; Prados, Ana] Univ Maryland Baltimore Cty, GEST, Baltimore, MD 21228 USA. EM mian.chin@nasa.gov RI Chin, Mian/J-8354-2012; Yu, Hongbin/C-6485-2008; Kahn, Ralph/D-5371-2012 OI Yu, Hongbin/0000-0003-4706-1575; Kahn, Ralph/0000-0002-5234-6359 NR 0 TC 0 Z9 0 U1 0 U2 2 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0016-7037 J9 GEOCHIM COSMOCHIM AC JI Geochim. Cosmochim. Acta PD JUN PY 2009 VL 73 IS 13 BP A219 EP A219 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 460YS UT WOS:000267229900451 ER PT J AU Goldblatt, C Matthews, AJ Claire, M Lenton, TM Watson, AJ Zahnle, KJ AF Goldblatt, Colin Matthews, Adrian J. Claire, Mark Lenton, Timothy M. Watson, Andrew J. Zahnle, Kevin J. TI There was probably more nitrogen in the Archean atmosphere - This would have helped resolve the Faint Young Sun paradox SO GEOCHIMICA ET COSMOCHIMICA ACTA LA English DT Meeting Abstract CT 19th Annual VM Goldschmidt Conference CY JUN 21, 2009 CL Davos, SWITZERLAND C1 [Goldblatt, Colin; Zahnle, Kevin J.] NASA, Ames Res Ctr, Space Sci & Astrobiol Div, Moffett Field, CA 94035 USA. [Matthews, Adrian J.; Lenton, Timothy M.; Watson, Andrew J.] Univ E Anglia, Sch Environm Sci, Norwich NR4 7TJ, Norfolk, England. [Claire, Mark] Univ Washington, Virtual Planetary Lab & Astrobiol Program, Seattle, WA 98195 USA. EM colin.goldblatt@nasa.gov RI Matthews, Adrian/A-6444-2011 OI Matthews, Adrian/0000-0003-0492-1168 NR 0 TC 1 Z9 1 U1 0 U2 5 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0016-7037 J9 GEOCHIM COSMOCHIM AC JI Geochim. Cosmochim. Acta PD JUN PY 2009 VL 73 IS 13 BP A446 EP A446 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 460YS UT WOS:000267229901123 ER PT J AU Haghighipour, N Hinse, T Steffen, J Agol, E AF Haghighipour, N. Hinse, T. Steffen, J. Agol, E. TI Implications of dynamical stability for the detection of Super-Earths via transit timing variation method SO GEOCHIMICA ET COSMOCHIMICA ACTA LA English DT Meeting Abstract CT 19th Annual VM Goldschmidt Conference CY JUN 21, 2009 CL Davos, SWITZERLAND C1 [Haghighipour, N.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. [Haghighipour, N.] Univ Hawaii, NASA, Astrobiol Inst, Honolulu, HI 96822 USA. [Hinse, T.] Armagh Observ, Armagh BT61 9DG, North Ireland. [Steffen, J.] Fermilab Natl Accelerator Lab, Batavia, IL 60510 USA. [Agol, E.] Univ Washington, Dept Phys & Astron, Seattle, WA 98105 USA. EM nader@ifa.hawaii.edu RI Agol, Eric/B-8775-2013 OI Agol, Eric/0000-0002-0802-9145 NR 0 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 0016-7037 J9 GEOCHIM COSMOCHIM AC JI Geochim. Cosmochim. Acta PD JUN PY 2009 VL 73 IS 13 BP A486 EP A486 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 460YS UT WOS:000267229901203 ER PT J AU Harley, RA Ban-Weiss, GA Kirchsetter, TW Lunden, MM Strawa, AW AF Harley, Robert A. Ban-Weiss, George A. Kirchsetter, Thomas W. Lunden, Melissa M. Strawa, Anthony W. TI Particulate matter optical properties and emission trends for gasoline and diesel vehicles SO GEOCHIMICA ET COSMOCHIMICA ACTA LA English DT Meeting Abstract CT 19th Annual VM Goldschmidt Conference CY JUN 21, 2009 CL Davos, SWITZERLAND C1 [Harley, Robert A.; Ban-Weiss, George A.] Univ Calif Berkeley, Dept Civil & Environm Engn, Berkeley, CA 94720 USA. [Kirchsetter, Thomas W.; Lunden, Melissa M.] Univ Calif Berkeley, Lawrence Berkeley Lab, Dept Atmospher Sci, Berkeley, CA 94720 USA. [Strawa, Anthony W.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. EM harley@ce.berkeley.edu; georgebw@me.berkeley.edu; twkirchstetter@lbl.gov; mmlunden@lbl.gov; anthony.w.strawa@nasa.gov RI Harley, Robert/C-9177-2016 OI Harley, Robert/0000-0002-0559-1917 NR 0 TC 0 Z9 0 U1 0 U2 5 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0016-7037 J9 GEOCHIM COSMOCHIM AC JI Geochim. Cosmochim. Acta PD JUN PY 2009 VL 73 IS 13 BP A494 EP A494 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 460YS UT WOS:000267229901220 ER PT J AU Heber, VS Vogel, N Wieler, R Burnett, DS AF Heber, V. S. Vogel, N. Wieler, R. Burnett, D. S. TI The composition of noble gases in the solar wind as collected by Genesis: A proxy for solar nebula composition SO GEOCHIMICA ET COSMOCHIMICA ACTA LA English DT Meeting Abstract CT 19th Annual VM Goldschmidt Conference CY JUN 21, 2009 CL Davos, SWITZERLAND C1 [Heber, V. S.] Univ Calif Los Angeles, Los Angeles, CA USA. [Vogel, N.; Wieler, R.] Swiss Fed Inst Technol, Zurich, Switzerland. [Burnett, D. S.] CALTECH, Jet Prop Lab, Pasadena, CA USA. EM heber@ess.ucla.edu; wieler@erdw.ethz.ch; burnett@gps.caltech.edu NR 4 TC 0 Z9 0 U1 0 U2 2 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0016-7037 J9 GEOCHIM COSMOCHIM AC JI Geochim. Cosmochim. Acta PD JUN PY 2009 VL 73 IS 13 BP A509 EP A509 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 460YS UT WOS:000267229901249 ER PT J AU Heimann, A Johnson, CM Beard, BL Valley, JW Spicuzza, MJ AF Heimann, A. Johnson, C. M. Beard, B. L. Valley, J. W. Spicuzza, M. J. TI The role of microbial processes in Banded Iron Formation (BIF) genesis as constrained by Fe, C, and O isotopes in BIF carbonates SO GEOCHIMICA ET COSMOCHIMICA ACTA LA English DT Meeting Abstract CT 19th Annual VM Goldschmidt Conference CY JUN 21, 2009 CL Davos, SWITZERLAND C1 [Heimann, A.; Johnson, C. M.; Beard, B. L.; Valley, J. W.; Spicuzza, M. J.] Univ Wisconsin, Madison, WI 53706 USA. [Heimann, A.; Johnson, C. M.; Beard, B. L.; Valley, J. W.; Spicuzza, M. J.] NASA, Astrobiol Inst, Washington, DC 20546 USA. EM aheimann@geology.wisc.edu RI Valley, John/B-3466-2011 OI Valley, John/0000-0003-3530-2722 NR 0 TC 1 Z9 1 U1 0 U2 7 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0016-7037 J9 GEOCHIM COSMOCHIM AC JI Geochim. Cosmochim. Acta PD JUN PY 2009 VL 73 IS 13 BP A513 EP A513 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 460YS UT WOS:000267229901257 ER PT J AU Huberty, JM Kita, NT Heck, PR Kozdon, R Fournelle, JH Xu, HF Valley, JW AF Huberty, Jason M. Kita, Noriko T. Heck, Philipp R. Kozdon, Reinhard Fournelle, John H. Xu, Huifang Valley, John W. TI Crystal orientation effects on bias of delta O-18 in magnetite by SIMS SO GEOCHIMICA ET COSMOCHIMICA ACTA LA English DT Meeting Abstract CT 19th Annual VM Goldschmidt Conference CY JUN 21, 2009 CL Davos, SWITZERLAND C1 Univ Wisconsin, Dept Geol & Geophys, NASA Astrobiol Inst, Madison, WI 53706 USA. Univ Wisconsin, Dept Geol & Geophys, Wisc SIMS, Madison, WI 53706 USA. EM jason@geology.wisc.edu RI Valley, John/B-3466-2011; Heck, Philipp/C-6092-2012; Kozdon, Reinhard/J-9468-2014 OI Valley, John/0000-0003-3530-2722; Kozdon, Reinhard/0000-0001-6347-456X NR 0 TC 2 Z9 2 U1 1 U2 2 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0016-7037 J9 GEOCHIM COSMOCHIM AC JI Geochim. Cosmochim. Acta PD JUN PY 2009 VL 73 IS 13 SU S BP A562 EP A562 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 460YS UT WOS:000267229901355 ER PT J AU Ichoku, C Chin, M Diehl, T Tan, Q AF Ichoku, Charles Chin, Mian Diehl, Thomas Tan, Qian TI Smoke source strength from satellite measurements of fire strength SO GEOCHIMICA ET COSMOCHIMICA ACTA LA English DT Meeting Abstract CT 19th Annual VM Goldschmidt Conference CY JUN 21, 2009 CL Davos, SWITZERLAND C1 [Ichoku, Charles; Chin, Mian; Diehl, Thomas; Tan, Qian] NASA GSFC, Atmospheres Lab, Greenbelt, MD 20771 USA. [Diehl, Thomas; Tan, Qian] Univ Maryland Baltimore Cty, GEST, Baltimore, MD 21228 USA. RI Ichoku, Charles/E-1857-2012 OI Ichoku, Charles/0000-0003-3244-4549 NR 0 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 0016-7037 J9 GEOCHIM COSMOCHIM AC JI Geochim. Cosmochim. Acta PD JUN PY 2009 VL 73 IS 13 BP A566 EP A566 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 460YS UT WOS:000267229901363 ER PT J AU Johnson, CM Yamaguchi, KE Poulson, SR Ohmoto, H Beard, BL AF Johnson, Clark M. Yamaguchi, Kosei E. Poulson, Simon R. Ohmoto, Hiroshi Beard, Brian L. TI Fe, S, and C isotopes record great microbial diversity in the Neoarchean SO GEOCHIMICA ET COSMOCHIMICA ACTA LA English DT Meeting Abstract CT 19th Annual VM Goldschmidt Conference CY JUN 21, 2009 CL Davos, SWITZERLAND C1 [Johnson, Clark M.; Beard, Brian L.] Univ Wisconsin, Madison, WI 53706 USA. [Johnson, Clark M.; Yamaguchi, Kosei E.; Ohmoto, Hiroshi; Beard, Brian L.] NASA, Astrobiol Inst, Washington, DC 20546 USA. [Poulson, Simon R.] Univ Nevada, Reno, NV 89557 USA. [Ohmoto, Hiroshi] Penn State Univ, University Pk, PA 16802 USA. EM clarkj@geology.wisc.edu NR 0 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 0016-7037 J9 GEOCHIM COSMOCHIM AC JI Geochim. Cosmochim. Acta PD JUN PY 2009 VL 73 IS 13 BP A600 EP A600 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 460YS UT WOS:000267229901432 ER PT J AU Johnson, M Meskhidze, N Solmon, F Fairlie, D Gasso, S AF Johnson, M. Meskhidze, N. Solmon, F. Fairlie, D. Gasso, S. TI Modeling mineral dust and dissolved iron deposition SO GEOCHIMICA ET COSMOCHIMICA ACTA LA English DT Meeting Abstract CT 19th Annual VM Goldschmidt Conference CY JUN 21, 2009 CL Davos, SWITZERLAND C1 [Johnson, M.; Meskhidze, N.] N Carolina State Univ, Raleigh, NC 27613 USA. [Solmon, F.] ASIC Theoret Phys, Trieste, Italy. [Fairlie, D.] NASA, Langley Res Ctr, Hampton, VA 23665 USA. [Gasso, S.] Goddard Earth Sci & Tech Ctr, Greenbelt, MD USA. EM nmeskhidze@ncsu.edu NR 3 TC 0 Z9 0 U1 1 U2 2 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0016-7037 J9 GEOCHIM COSMOCHIM AC JI Geochim. Cosmochim. Acta PD JUN PY 2009 VL 73 IS 13 BP A601 EP A601 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 460YS UT WOS:000267229901434 ER PT J AU Kanakidou, M Myriokefalitakis, S Tsigaridis, K Daskalakis, N AF Kanakidou, M. Myriokefalitakis, S. Tsigaridis, K. Daskalakis, N. TI Global sources of organic aerosols in the atmosphere: Reconciling model results with observations SO GEOCHIMICA ET COSMOCHIMICA ACTA LA English DT Meeting Abstract CT 19th Annual VM Goldschmidt Conference CY JUN 21, 2009 CL Davos, SWITZERLAND C1 [Kanakidou, M.; Myriokefalitakis, S.; Daskalakis, N.] Univ Crete, Environm Chem Proc Lab, Dept Chem, Iraklion 71003, Greece. [Tsigaridis, K.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA. EM mariak@chemistry.uoc.gr RI Kanakidou, Maria/D-7882-2012; Tsigaridis, Kostas/K-8292-2012; Daskalakis, Nikos/B-9632-2014; Myriokefalitakis, Stylianos/J-3701-2014 OI Kanakidou, Maria/0000-0002-1724-9692; Tsigaridis, Kostas/0000-0001-5328-819X; Daskalakis, Nikos/0000-0002-2409-0392; Myriokefalitakis, Stylianos/0000-0002-1541-7680 NR 0 TC 0 Z9 0 U1 0 U2 2 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0016-7037 J9 GEOCHIM COSMOCHIM AC JI Geochim. Cosmochim. Acta PD JUN PY 2009 VL 73 IS 13 BP A619 EP A619 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 460YS UT WOS:000267229901470 ER PT J AU Keene, WC Long, MS Sander, R Kieber, DJ Maring, H Pszenny, AAP AF Keene, W. C. Long, M. S. Sander, R. Kieber, D. J. Maring, H. Pszenny, A. A. P. TI Marine aerosol production, chemical evolution, and feedbacks over the open ocean SO GEOCHIMICA ET COSMOCHIMICA ACTA LA English DT Meeting Abstract CT 19th Annual VM Goldschmidt Conference CY JUN 21, 2009 CL Davos, SWITZERLAND C1 [Keene, W. C.; Long, M. S.] Univ Virginia, Charlottesville, VA 22904 USA. [Sander, R.] Max Planck Inst Chem, D-55020 Mainz, Germany. [Kieber, D. J.] SUNY, Syracuse, NY 13210 USA. [Maring, H.] NASA, Radiat Sci Program, Washington, DC 20546 USA. [Pszenny, A. A. P.] Univ New Hampshire, Durham, NH 03824 USA. EM wck@virginia.edu RI Sander, Rolf/A-5725-2011 OI Sander, Rolf/0000-0001-6479-2092 NR 0 TC 0 Z9 0 U1 1 U2 4 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0016-7037 J9 GEOCHIM COSMOCHIM AC JI Geochim. Cosmochim. Acta PD JUN PY 2009 VL 73 IS 13 SU S BP A633 EP A633 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 460YS UT WOS:000267229901497 ER PT J AU Konhauser, KO Pecoits, E Lalonde, SV Papineau, D Nisbet, EG Barley, ME Arndt, NT Zahnle, K Kamber, BS AF Konhauser, K. O. Pecoits, E. Lalonde, S. V. Papineau, D. Nisbet, E. G. Barley, M. E. Arndt, N. T. Zahnle, K. Kamber, B. S. TI Oceanic Nickel depletion and a methanogen famine before the Great Oxidation Event SO GEOCHIMICA ET COSMOCHIMICA ACTA LA English DT Meeting Abstract CT 19th Annual VM Goldschmidt Conference CY JUN 21, 2009 CL Davos, SWITZERLAND C1 [Konhauser, K. O.; Pecoits, E.; Lalonde, S. V.] Univ Alberta, Dept Earth & Atmospher Sci, Edmonton, AB T6G 2E3, Canada. [Papineau, D.] Carnegie Inst Washington, Washington, DC 20005 USA. [Barley, M. E.] Univ Western Australia, Crawley, Australia. [Nisbet, E. G.] Royal Holloway Univ London, London, England. [Arndt, N. T.] Univ Grenoble 1, Grenoble, France. [Zahnle, K.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Kamber, B. S.] Laurentian Univ, Sudbury, ON P3E 2C6, Canada. EM kurtk@ualberta.ca RI Lalonde, Stefan/I-8879-2014 OI Lalonde, Stefan/0000-0003-1318-2280 NR 0 TC 2 Z9 2 U1 1 U2 12 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0016-7037 J9 GEOCHIM COSMOCHIM AC JI Geochim. Cosmochim. Acta PD JUN PY 2009 VL 73 IS 13 BP A678 EP A678 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 460YS UT WOS:000267229901588 ER PT J AU Koren, I Feingold, G Remer, LA Martins, JV AF Koren, Ilan Feingold, Graham Remer, Lorraine A. Martins, J. Vanderlei TI How interactions between clouds and aerosols depend on scale SO GEOCHIMICA ET COSMOCHIMICA ACTA LA English DT Meeting Abstract CT 19th Annual VM Goldschmidt Conference CY JUN 21, 2009 CL Davos, SWITZERLAND C1 [Koren, Ilan] Weizmann Inst Sci, IL-76100 Rehovot, Israel. [Feingold, Graham] NOAA, ESRL, Boulder, CO 80305 USA. [Remer, Lorraine A.] NASA, Goddard Space Flight Ctr, Atmospheres Lab, Greenbelt, MD 20771 USA. [Martins, J. Vanderlei] Univ Maryland Baltimore Cty, Dept Phys, Baltimore, MD 21228 USA. [Martins, J. Vanderlei] Univ Maryland Baltimore Cty, Joint Ctr Earth Syst Technol, Baltimore, MD 21228 USA. EM Ilan.koren@weizmann.ac.il; Graham.Feingold@noaa.gov; lorraine.a.remer@nasa.gov; martins@umbc.edu RI Feingold, Graham/B-6152-2009; Koren, Ilan/K-1417-2012 OI Koren, Ilan/0000-0001-6759-6265 NR 0 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 0016-7037 J9 GEOCHIM COSMOCHIM AC JI Geochim. Cosmochim. Acta PD JUN PY 2009 VL 73 IS 13 BP A682 EP A682 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 460YS UT WOS:000267229901596 ER PT J AU Marais, DJD AF Marais, David J. Des TI Hints of habitable environments on Mars challenge our studies of Mars-Analog sites on Earth SO GEOCHIMICA ET COSMOCHIMICA ACTA LA English DT Meeting Abstract CT 19th Annual VM Goldschmidt Conference CY JUN 21, 2009 CL Davos, SWITZERLAND C1 [Marais, David J. Des] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. EM David.J.DesMarais@nasa.gov NR 0 TC 0 Z9 0 U1 0 U2 0 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0016-7037 J9 GEOCHIM COSMOCHIM AC JI Geochim. Cosmochim. Acta PD JUN PY 2009 VL 73 IS 13 BP A285 EP A285 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 460YS UT WOS:000267229900582 ER PT J AU Menon, S Koch, D Beig, G Orlikowski, D AF Menon, S. Koch, D. Beig, G. Orlikowski, D. TI Aerosol influence on decadal changes in precipitation and snow cover over Asia SO GEOCHIMICA ET COSMOCHIMICA ACTA LA English DT Meeting Abstract CT 19th Annual VM Goldschmidt Conference CY JUN 21, 2009 CL Davos, SWITZERLAND C1 [Menon, S.] Univ Calif Berkeley, Lawrence Berkeley Lab, Berkeley, CA 94720 USA. [Koch, D.] Columbia Univ, NASA GISS, New York, NY USA. [Beig, G.] Indian Inst Trop Meteorol, Pune, Maharashtra, India. [Orlikowski, D.] Lawrence Livermore Natl Lab, Livermore, CA USA. EM smenon@lbl.gov NR 0 TC 0 Z9 0 U1 0 U2 0 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0016-7037 J9 GEOCHIM COSMOCHIM AC JI Geochim. Cosmochim. Acta PD JUN PY 2009 VL 73 IS 13 BP A870 EP A870 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 460YS UT WOS:000267229902199 ER PT J AU Murray, AE Fritsen, CH Kenig, F Mckay, CM McKnight, DM Cawley, K Doran, PT AF Murray, A. E. Fritsen, C. H. Kenig, F. McKay, C. M. McKnight, D. M. Cawley, K. Doran, P. T. TI Life in the ice cover and underlying cold brines of Lake Vida, Antarctica SO GEOCHIMICA ET COSMOCHIMICA ACTA LA English DT Meeting Abstract CT 19th Annual VM Goldschmidt Conference CY JUN 21, 2009 CL Davos, SWITZERLAND C1 [Murray, A. E.; Fritsen, C. H.] Univ Nevada, Desert Res Inst, Reno, NV 89506 USA. [Kenig, F.; Doran, P. T.] Univ Illinois, Chicago, IL USA. [McKay, C. M.] NASA Ames, Moffett Field, CA USA. [McKnight, D. M.; Cawley, K.] Univ Colorado, INSTAAR, Boulder, CO 80309 USA. EM alison.murray@dri.edu; cfritsen@dri.edu; fkenig@uic.edu; christopher.mckay@nasa.gov; diane.mcknight@Colorado.edu; kaelin.cawley@colorado.edu; pdoran@uic.edu NR 0 TC 0 Z9 0 U1 3 U2 13 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0016-7037 J9 GEOCHIM COSMOCHIM AC JI Geochim. Cosmochim. Acta PD JUN PY 2009 VL 73 IS 13 SU S BP A922 EP A922 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 460YS UT WOS:000267229902303 ER PT J AU Ohmoto, H AF Ohmoto, Hiroshi TI Redox evolution of volcanic gas through geologic time SO GEOCHIMICA ET COSMOCHIMICA ACTA LA English DT Meeting Abstract CT 19th Annual VM Goldschmidt Conference CY JUN 21, 2009 CL Davos, SWITZERLAND C1 [Ohmoto, Hiroshi] Penn State Univ, NASA, Astrobiol Inst, University Pk, PA 16802 USA. [Ohmoto, Hiroshi] Penn State Univ, Dept Geosci, University Pk, PA 16802 USA. EM ohmoto@geosc.psu.edu NR 0 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 0016-7037 J9 GEOCHIM COSMOCHIM AC JI Geochim. Cosmochim. Acta PD JUN PY 2009 VL 73 IS 13 BP A965 EP A965 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 460YS UT WOS:000267229902389 ER PT J AU Papineau, D De Gregorio, BT Fries, MD Steele, A Stroud, RM Wang, J Mojzsis, SJ Konhauser, KO Pecoits, E Cody, GD Fogel, ML AF Papineau, D. De Gregorio, B. T. Fries, M. D. Steele, A. Stroud, R. M. Wang, J. Mojzsis, S. J. Konhauser, K. O. Pecoits, E. Cody, G. D. Fogel, M. L. TI Carbonaceous material associated with apatite in the Akilia Qp rock SO GEOCHIMICA ET COSMOCHIMICA ACTA LA English DT Meeting Abstract CT 19th Annual VM Goldschmidt Conference CY JUN 21, 2009 CL Davos, SWITZERLAND C1 [Papineau, D.; Steele, A.; Wang, J.; Cody, G. D.; Fogel, M. L.] Carnegie Inst Washington, Washington, DC 20015 USA. [De Gregorio, B. T.; Stroud, R. M.] USN, Res Lab, Div Mat Sci & Technol, Washington, DC 20375 USA. [Fries, M. D.] NASA, Jet Prop Lab, Pasadena, CA USA. [Mojzsis, S. J.] Univ Colorado, Dept Geol Sci, Boulder, CO 80309 USA. [Konhauser, K. O.; Pecoits, E.] Univ Alberta, Dept Earth Sci, Edmonton, AB, Canada. EM dpapineau@ciw.edu RI De Gregorio, Bradley/B-8465-2008 OI De Gregorio, Bradley/0000-0001-9096-3545 NR 0 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 0016-7037 J9 GEOCHIM COSMOCHIM AC JI Geochim. Cosmochim. Acta PD JUN PY 2009 VL 73 IS 13 BP A991 EP A991 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 460YS UT WOS:000267229902442 ER PT J AU Remer, LA Kahn, RA Koren, I AF Remer, L. A. Kahn, R. A. Koren, I. TI Aerosol indirect effects from satellite: Skeptics vs. optimists SO GEOCHIMICA ET COSMOCHIMICA ACTA LA English DT Meeting Abstract CT 19th Annual VM Goldschmidt Conference CY JUN 21, 2009 CL Davos, SWITZERLAND C1 [Remer, L. A.; Kahn, R. A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Koren, I.] Weizmann Inst Sci, IL-76100 Rehovot, Israel. RI Koren, Ilan/K-1417-2012; Kahn, Ralph/D-5371-2012 OI Koren, Ilan/0000-0001-6759-6265; Kahn, Ralph/0000-0002-5234-6359 NR 0 TC 0 Z9 0 U1 0 U2 2 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0016-7037 J9 GEOCHIM COSMOCHIM AC JI Geochim. Cosmochim. Acta PD JUN PY 2009 VL 73 IS 13 BP A1088 EP A1088 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 460YS UT WOS:000267229902634 ER PT J AU Tobler, DJ Benning, LG Fogel, ML Glamoclija, A Kerr, L Steele, A Amundsen, HEF Eigenbrode, JL AF Tobler, D. J. Benning, L. G. Fogel, M. L. Glamoclija, A. Kerr, L. Steele, A. Amundsen, H. E. F. Eigenbrode, J. L. CA 2008 AMASE Team TI Signatures of Life in Ice (SLIce): An analog study for in situ detection of biosignatures elsewhere SO GEOCHIMICA ET COSMOCHIMICA ACTA LA English DT Meeting Abstract CT 19th Annual VM Goldschmidt Conference CY JUN 21, 2009 CL Davos, SWITZERLAND C1 [Tobler, D. J.; Eigenbrode, J. L.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Tobler, D. J.; Eigenbrode, J. L.] Goddard Ctr Astrobiol, Greenbelt, MD 20771 USA. [Benning, L. G.] Univ Leeds, Sch Earth & Environm, Earth & Biosphere Inst, Leeds LS2 9JT, W Yorkshire, England. [Fogel, M. L.; Glamoclija, A.; Kerr, L.; Steele, A.] Carnegie Inst Washington, Geophys Lab, Washington, DC 20015 USA. [Amundsen, H. E. F.] Earth & Planetary Explorat Serv, N-0364 Oslo, Norway. EM Jennifer.Eigenbrode@nasa.gov RI Eigenbrode, Jennifer/D-4651-2012; Tobler, Dominique/G-3213-2012 OI Tobler, Dominique/0000-0001-8532-1855 NR 0 TC 0 Z9 0 U1 1 U2 5 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0016-7037 J9 GEOCHIM COSMOCHIM AC JI Geochim. Cosmochim. Acta PD JUN PY 2009 VL 73 IS 13 BP A1333 EP A1333 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 460YS UT WOS:000267229903353 ER PT J AU Touboul, M Kleine, T Bourdon, B Nyquist, L Shih, CY AF Touboul, M. Kleine, T. Bourdon, B. Nyquist, L. Shih, C. -Y. TI New Sm-146-Nd-142 data for lunar rocks SO GEOCHIMICA ET COSMOCHIMICA ACTA LA English DT Meeting Abstract CT 19th Annual VM Goldschmidt Conference CY JUN 21, 2009 CL Davos, SWITZERLAND ID MOON; DIFFERENTIATION; MANTLE C1 [Touboul, M.; Kleine, T.; Bourdon, B.] Swiss Fed Inst Technol, Inst Isotope Geochem & Mineral Resources, Zurich, Switzerland. [Nyquist, L.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. [Shih, C. -Y.] Jacobs Sverdrup, Houston, TX USA. EM touboul@erdw.ethz.ch RI Bourdon, Bernard/A-3303-2008 NR 5 TC 0 Z9 0 U1 0 U2 2 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0016-7037 J9 GEOCHIM COSMOCHIM AC JI Geochim. Cosmochim. Acta PD JUN PY 2009 VL 73 IS 13 SU S BP A1342 EP A1342 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 460YS UT WOS:000267229903372 ER PT J AU Tsigaridis, K Kanakidou, M Myriokefalitakis, S Perakis, L AF Tsigaridis, K. Kanakidou, M. Myriokefalitakis, S. Perakis, L. TI Simplicity versus accuracy in global secondary organic aerosol modeling SO GEOCHIMICA ET COSMOCHIMICA ACTA LA English DT Meeting Abstract CT 19th Annual VM Goldschmidt Conference CY JUN 21, 2009 CL Davos, SWITZERLAND C1 [Tsigaridis, K.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA. [Kanakidou, M.; Myriokefalitakis, S.; Perakis, L.] Univ Crete, Environm Chem Proc Lab, Dept Chem, Iraklion, Greece. EM ktsigaridis@giss.nasa.gov; mariak@chemistry.uoc.gr; stelios@chemistry.uoc.gr; perakis@nah.gr RI Kanakidou, Maria/D-7882-2012; Tsigaridis, Kostas/K-8292-2012; Myriokefalitakis, Stylianos/J-3701-2014 OI Kanakidou, Maria/0000-0002-1724-9692; Tsigaridis, Kostas/0000-0001-5328-819X; Myriokefalitakis, Stylianos/0000-0002-1541-7680 NR 0 TC 0 Z9 0 U1 0 U2 2 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0016-7037 J9 GEOCHIM COSMOCHIM AC JI Geochim. Cosmochim. Acta PD JUN PY 2009 VL 73 IS 13 BP A1349 EP A1349 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 460YS UT WOS:000267229903386 ER PT J AU Villanueva, GL Mumma, MJ Novak, RE AF Villanueva, G. L. Mumma, M. J. Novak, R. E. TI Strong release of methane on Mars: Evidence of biology or geology? SO GEOCHIMICA ET COSMOCHIMICA ACTA LA English DT Meeting Abstract CT 19th Annual VM Goldschmidt Conference CY JUN 21, 2009 CL Davos, SWITZERLAND C1 [Villanueva, G. L.; Mumma, M. J.] NASA, Goddard Space Flight Ctr, Solar Syst Explorat Div Code 693, Greenbelt, MD 20771 USA. [Villanueva, G. L.] Catholic Univ Amer, Dept Phys, Washington, DC 20008 USA. [Novak, R. E.] Iona Coll, Dept Phys, New Rochelle, NY 10801 USA. EM geronimo.villanueva@nasa.gov RI mumma, michael/I-2764-2013 NR 3 TC 7 Z9 7 U1 0 U2 5 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0016-7037 J9 GEOCHIM COSMOCHIM AC JI Geochim. Cosmochim. Acta PD JUN PY 2009 VL 73 IS 13 BP A1384 EP A1384 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 460YS UT WOS:000267229903456 ER PT J AU Vogel, N Heber, VS Baur, H Burnett, DS Wieler, R AF Vogel, N. Heber, V. S. Baur, H. Burnett, D. S. Wieler, R. TI Solar wind Ar, Kr, and Xe abundances deduced from Genesis targets SO GEOCHIMICA ET COSMOCHIMICA ACTA LA English DT Meeting Abstract CT 19th Annual VM Goldschmidt Conference CY JUN 21, 2009 CL Davos, SWITZERLAND ID KRYPTON; XENON C1 [Vogel, N.; Baur, H.; Wieler, R.] Swiss Fed Inst Technol, IGMR, Zurich, Switzerland. [Heber, V. S.] Univ Calif Los Angeles, EPS, Los Angeles, CA USA. [Burnett, D. S.] CALTECH, Jet Prop Lab, Pasadena, CA USA. EM nadia.vogel@erdw.ethz.ch; heber@ess.ucla.edu; burnett@gps.caltech.edu RI Wieler, Rainer/A-1355-2010 OI Wieler, Rainer/0000-0001-5666-7494 NR 9 TC 0 Z9 0 U1 0 U2 3 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0016-7037 J9 GEOCHIM COSMOCHIM AC JI Geochim. Cosmochim. Acta PD JUN PY 2009 VL 73 IS 13 BP A1391 EP A1391 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 460YS UT WOS:000267229903469 ER PT J AU Wierzchos, J De Los Rios, A Davila, AF Camara, B Valea, S Esteve, I Sole, A Roldan, M Rodriguez, R Sanchez-Almazo, IM McKay, CP Ascaso, C AF Wierzchos, J. De Los Rios, A. Davila, A. F. Camara, B. Valea, S. Esteve, I. Sole, A. Roldan, M. Rodriguez, R. Sanchez-Almazo, I. M. McKay, C. P. Ascaso, C. TI Primary producers in extreme arid environment of the Atacama Desert: Where, how and when? SO GEOCHIMICA ET COSMOCHIMICA ACTA LA English DT Meeting Abstract CT 19th Annual VM Goldschmidt Conference CY JUN 21, 2009 CL Davos, SWITZERLAND C1 [Wierzchos, J.; De Los Rios, A.; Camara, B.; Valea, S.; Rodriguez, R.; Ascaso, C.] CSIC, Inst Recursos Nat, E-28006 Madrid, Spain. [Davila, A. F.; McKay, C. P.] NASA, Ames Res Ctr, Moffett Field, CA 94087 USA. [Esteve, I.; Sole, A.; Roldan, M.] Univ Autonoma Barcelona, E-08193 Barcelona, Spain. [Sanchez-Almazo, I. M.] Univ Granada, CEAMA, Granada 18006, Spain. EM j.wierzchos@ccma.csic.es RI Wierzchos, Jacek/F-7036-2011; Ascaso, Carmen/F-5369-2011; Davila, Alfonso/A-2198-2013; Sole, Antonio/L-4195-2014; Camara Gallego, Beatriz/H-6407-2015 OI Wierzchos, Jacek/0000-0003-3084-3837; Ascaso, Carmen/0000-0001-9665-193X; Davila, Alfonso/0000-0002-0977-9909; Sole, Antonio/0000-0002-1151-319X; Camara Gallego, Beatriz/0000-0003-4945-3134 NR 3 TC 0 Z9 0 U1 1 U2 2 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0016-7037 J9 GEOCHIM COSMOCHIM AC JI Geochim. Cosmochim. Acta PD JUN PY 2009 VL 73 IS 13 BP A1439 EP A1439 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 460YS UT WOS:000267229903566 ER PT J AU Yamaguchi, KE Kato, Y Nakamura, K Suzuki, K Watanabe, Y Nedachi, M Ohmoto, H AF Yamaguchi, Kosei E. Kato, Yasuhiro Nakamura, Kentaro Suzuki, Katsuhiko Watanabe, Yumiko Nedachi, Munetomo Ohmoto, Hiroshi TI REE plus Y geochemistry of the 3.46 Ga Marble Bar Chert recovered by the Archean Biosphere Drilling Project (ABDP) SO GEOCHIMICA ET COSMOCHIMICA ACTA LA English DT Meeting Abstract CT 19th Annual VM Goldschmidt Conference CY JUN 21, 2009 CL Davos, SWITZERLAND C1 [Yamaguchi, Kosei E.] Toho Univ, Dept Chem, Geochem Lab, Chiba 2748510, Japan. [Yamaguchi, Kosei E.; Watanabe, Yumiko; Ohmoto, Hiroshi] NASA Astrobiol Inst, Washington, DC USA. [Kato, Yasuhiro] Univ Tokyo, Dept Syst Innovat, Tokyo, Japan. [Nakamura, Kentaro] Univ Tokyo, Frontier Res Ctr Energy & Resources, Tokyo, Japan. [Watanabe, Yumiko; Ohmoto, Hiroshi] Penn State Univ, Dept Geosci, University Pk, PA 16802 USA. [Nedachi, Munetomo] Kagoshima Univ, Dept Phys, Kagoshima 890, Japan. EM kosei@chem.sci.toho-u.ac.jp NR 0 TC 0 Z9 0 U1 0 U2 0 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0016-7037 J9 GEOCHIM COSMOCHIM AC JI Geochim. Cosmochim. Acta PD JUN PY 2009 VL 73 IS 13 BP A1469 EP A1469 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 460YS UT WOS:000267229903625 ER PT J AU Yoshizaki, M Suzuki, K Shibuya, T Shimizu, K Nakamura, K Yamaguchi, KE Yamamoto, S Omori, S Takai, K Maruyama, S AF Yoshizaki, Motoko Suzuki, Katsuhiko Shibuya, Takazo Shimizu, Kenji Nakamura, Kentaro Yamaguchi, Kosei E. Yamamoto, Shinji Omori, Soichi Takai, Ken Maruyama, Shigenori TI Experimental study on hydrogen production through hydrothermal alteration of komatiite glass SO GEOCHIMICA ET COSMOCHIMICA ACTA LA English DT Meeting Abstract CT 19th Annual VM Goldschmidt Conference CY JUN 21, 2009 CL Davos, SWITZERLAND C1 [Yoshizaki, Motoko; Yamamoto, Shinji; Omori, Soichi; Maruyama, Shigenori] Tokyo Tech, Dept Earth & Planet Sci, Tokyo, Japan. [Yoshizaki, Motoko; Suzuki, Katsuhiko; Shibuya, Takazo; Shimizu, Kenji; Nakamura, Kentaro; Yamaguchi, Kosei E.; Takai, Ken] JAMSTEC, Precam Ecosys Lab, Yokosuka, Kanagawa 2370061, Japan. [Suzuki, Katsuhiko; Shimizu, Kenji] JAMSTEC, IFREE, Yokosuka, Kanagawa 2370061, Japan. [Suzuki, Katsuhiko; Shimizu, Kenji] Univ Tokyo, Fac Engineer, Tokyo, Japan. [Nakamura, Kentaro; Takai, Ken] JAMSTEC, XBR, Yokosuka, Kanagawa 2370061, Japan. [Yamaguchi, Kosei E.] Toho Univ, Dept Chem, Funabashi, Chiba 2748510, Japan. [Yamaguchi, Kosei E.] NASA Astrobiol Inst, Washington, DC USA. EM katz@jamstec.go.jp RI Maruyama, Shigenori/C-8288-2009 NR 0 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 0016-7037 J9 GEOCHIM COSMOCHIM AC JI Geochim. Cosmochim. Acta PD JUN PY 2009 VL 73 IS 13 SU S BP A1488 EP A1488 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 460YS UT WOS:000267229903663 ER PT J AU Wu, XP Blom, RG Ivins, ER Oyafuso, FA Zhong, M AF Wu, Xiaoping Blom, Ronald G. Ivins, Erik R. Oyafuso, Fabiano A. Zhong, Min TI Improved inverse and probabilistic methods for geophysical applications of GRACE gravity data SO GEOPHYSICAL JOURNAL INTERNATIONAL LA English DT Article DE Inverse theory; Satellite geodesy; Time variable gravity ID FIELD; VARIABILITY; MODELS AB Mapping time-varying gravity via satellite-to-satellite tracking systems holds great potential as a new way to monitor the Earth's global climate system. Measurement noises and systematic deficiencies in sampling, both in time and space, cause global geoid or surface mass solutions to have a structured spherical harmonic error spectrum, with strong degree and order dependences and cross-correlations. To extract average values of geoid or surface mass variations around global gridpoints on Earth's surface and over various geographic regions, both the shape of the averaging kernel and the resulting average uncertainties must be considered quantitatively and statistically. We investigate two methods of the Backus and Gilbert continuous geophysical inverse formalism for optimal averages around points on Earth's surface. The first averaging kernel optimally approximates the Dirac-delta function. With an equivalent measure of deviation from the Dirac-delta function, the optimal average has greater (up to 2.6 times) accuracy than does the most widely used isotropic Gaussian filter for GRACE analysis. The second method was crafted to decrease the kernel weight as the distance from the point of interest increases. A new method is presented to use a modified Gaussian averaging kernel that reduces average uncertainties with minimum loss of resolution. The modified method has some advantages over using the kernel that optimally approximates the Dirac-d function. Both methods are computationally efficient and are applied to simulated and real GRACE data to compute improved averages around fine-resolution global gridpoints and used with non-diagonal covariance matrices to intelligently reduce effects of correlated errors. The optimal probabilistic method of least squares with a priori information is discussed in the spherical harmonic domain. The property of optimality will be preserved when the estimates are mapped to the geographic domain for spatial averages. A regionally-bounded Gaussian a priori function is derived in the spherical harmonic domain to better represent different change regimes separated by major geographic boundaries. We also introduce an algorithm to derive the optimal regional average incorporating a constraint such that the average weight over the region is unity. Applications of such more realistic a priori information (and/or constraint) can produce improved average estimates using satellite gravity data. C1 [Wu, Xiaoping; Blom, Ronald G.; Ivins, Erik R.; Oyafuso, Fabiano A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Zhong, Min] Chinese Acad Sci, Inst Geodesy & Geophys, Wuhan 430077, Peoples R China. RP Wu, XP (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr,M-S 238-600, Pasadena, CA 91109 USA. EM Xiaoping.Wu@jpl.nasa.gov RI yu, yan/C-2322-2012 FU Chinese National Sciences Foundation [406442042] FX Part of this work was carried out at the Jet Propulsion Laboratory (JPL), California Institute of Technology, under a contract with the National Aeronautics and Space Administration (NASA) and funded through NASA's Earth Surface and Interior programme and the internal Research and Technology Development (R&TD) programme. Partial support was also provided by Chinese National Sciences Foundation through grant 406442042. We thank Srinivas Bettadpur and John Ries of CSR for providing a full monthly GRACE error covariance matrix, Danan Dong, Richard Gross, Angelyn Moore, Susan Owen of JPL for contributions in processing the GPS data and discussions. We are also grateful to Ernst Schrama, Richard Holme, and an anonymous reviewer for their helpful comments which improved this paper. NR 33 TC 8 Z9 8 U1 0 U2 7 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0956-540X J9 GEOPHYS J INT JI Geophys. J. Int. PD JUN PY 2009 VL 177 IS 3 BP 865 EP 877 DI 10.1111/j.1365-246X.2009.04141.x PG 13 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 445BS UT WOS:000266025200004 ER PT J AU Ko, KS Lee, JS Kim, JG Lee, J AF Ko, Kyung-Seok Lee, Jin-Soo Kim, Jae-Gon Lee, Jeonghoon TI Assessments of natural and anthropogenic controls on the spatial distribution of stream water quality in Southeastern Korea SO GEOSCIENCES JOURNAL LA English DT Article DE hydrogeochemical; geostatistical; variographic; natural and anthropogenic; mineralization; cokriging ID REGIONAL GEOCHEMICAL SURVEY; MINERAL EXPLORATION; OUACHITA MOUNTAINS; USA; DENSITY AB Hydrogeochemical and geostatistical analyses were conducted to evaluate natural and anthropogenic effects using stream water data of Southeastern Korea acquired through the Hydrogeochemical Survey Program of the Korea Institute of Geoscience & Mineral Resources. The results of a variographic analysis of the spatial structure of stream water quality show that the semivarigrams of Ca, Mg, and HCO(3) have similar patterns and regional distributions, reflecting the same geogenic source of Paleozoic, Tertiary, and Cretaceous sedimentary rocks. Although Ca and Mg originated from Paleozoic sedimentary rocks, the distribution of Mg is significantly different from that of Ca due to the presence of dolomite in northeastern area of Korea, which enhances the Mg concentration in stream water. Studies of mineralization and acid mine drainage resulting from previous mining activities reveal a high Ba in sedimentary rock from of Kyongsang basin, as well as anomalous concentration of Al, Fe, and SO(4) in the Ogcheon and Tabaeksan mineralization areas. Saturation indices of barite determined using average Ba and SO(4) concentrations in stream water suggest the existence of barite mineralization deposits in sedimentary rock of Kyongsang Group. Na, Cl, K, NO(3), and Cl, exhibit effects of anthropogenic and marine sources in the stream water, with increasing values near residential, agricultural, and coastal areas. Cokriging analyses employing Ca-HCO(3), Ca-Sr, Ba-SO(4), and Na-Cl also revealed the nature of bedrock geology, mineralization, and anthropogenic and marine sources. C1 [Ko, Kyung-Seok; Lee, Jin-Soo; Kim, Jae-Gon] Korea Inst Geosci & Mineral Resources, Taejon 305350, South Korea. [Lee, Jeonghoon] CALTECH, Jet Prop Lab, Pasadena, CA 91101 USA. RP Ko, KS (reprint author), Korea Inst Geosci & Mineral Resources, Taejon 305350, South Korea. EM kyungsok@kigam.re.kr RI Lee, Jeonghoon/C-7354-2008; Lee, Jeonghoon/E-8116-2010 OI Lee, Jeonghoon/0000-0002-1256-4431 FU Ministry of Knowledge Economy of Korea [09-3414] FX This research was supported by the Basic Research Project (09-3414) of the Korea Institute of Geoscience and Mineral Resources ( KIGAM) funded by the Ministry of Knowledge Economy of Korea. The research described in this paper was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. NR 25 TC 2 Z9 2 U1 0 U2 3 PU SPRINGER HEIDELBERG PI HEIDELBERG PA TIERGARTENSTRASSE 17, D-69121 HEIDELBERG, GERMANY SN 1226-4806 J9 GEOSCI J JI Geosci. J. PD JUN PY 2009 VL 13 IS 2 BP 191 EP 200 DI 10.1007/s12303-009-0019-z PG 10 WC Geosciences, Multidisciplinary SC Geology GA 462OV UT WOS:000267366400010 ER PT J AU Mouginot, J Kofman, W Safaeinili, A Grima, C Herique, A Plaut, JJ AF Mouginot, J. Kofman, W. Safaeinili, A. Grima, C. Herique, A. Plaut, J. J. TI MARSIS surface reflectivity of the south residual cap of Mars SO ICARUS LA English DT Article DE Radar observations; Mars; Polar caps; Ices ID POLAR LAYERED DEPOSITS; RADAR SOUNDINGS; CO2 FROST; IONOSPHERE; SUBSURFACE; FEATURES AB The south residual cap of Mars is commonly described as a thin and bright layer of CO2-ice. The Mars Advanced Radar for Subsurface and lonospheric Sounding (MARSIS) is a low-frequency radar on board Mars Express operating at the wavelength between 55 and 230 m in vacuum. The reflection of the radar wave on a stratified medium like the residual cap can generate interferences, causing weaker surface reflections compared to reflections from a pure water ice surface. In order to understand this anomalous low reflectivity, we propose a stratified medium model, which allows us to estimate both the thickness and the dielectric constant of the optically thin slab. First, we consider the residual cap as single unit and show that the decrease in the reflected echo strength is well explained by a mean thickness of 11 m and a mean dielectric constant of 2.2. This value of dielectric constant is close to the experimental value 2.12 for pure CO2-ice. Second, we study the spatial variability of the radar surface reflectivity. We observe that the reflectivity is not homogeneous over the residual cap. This heterogeneity can be modeled either by variable thickness or variable dielectric constant. The surface reflectivity shows that two different units comprise the residual cap, one central unit with high reflectivity and surrounding, less reflective units. (C) 2009 Elsevier Inc. All rights reserved. C1 [Mouginot, J.; Kofman, W.; Grima, C.; Herique, A.] CNRS, UJF, Lab Planetol Grenoble, F-38041 Grenoble, France. [Safaeinili, A.; Plaut, J. J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Mouginot, J (reprint author), 122 Rue de la Piscine, F-38000 Grenoble, France. EM jeremie.mouginot@obs.ujf-grenoble.fr; wlodek.kofman@obs.ujf-grenoble.fr; ali.safaeinili@jpl.nasa.gov; cyril.grima@obs.ujf-grenoble.fr; alain.herique@obs.ujf-grenoble.fr; plaut@jpl.nasa.gov RI Kofman, Wlodek/C-4556-2008; Grima, Cyril/E-9800-2013; Mouginot, Jeremie/G-7045-2015; Herique, Alain/E-7210-2017 OI Grima, Cyril/0000-0001-7135-3055; Herique, Alain/0000-0003-3699-883X NR 28 TC 12 Z9 13 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 EI 1090-2643 J9 ICARUS JI Icarus PD JUN PY 2009 VL 201 IS 2 BP 454 EP 459 DI 10.1016/j.icarus.2009.01.009 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 446NW UT WOS:000266129300005 ER PT J AU White, OL Safaeinili, A Plaut, JJ Stofan, ER Clifford, SM Farrell, WM Heggy, E Picardi, G AF White, Oliver L. Safaeinili, Ali Plaut, Jeffrey J. Stofan, Ellen R. Clifford, Stephen M. Farrell, William M. Heggy, Essam Picardi, Giovanni TI MARSIS radar sounder observations in the vicinity of Ma'adim Vallis, Mars SO ICARUS LA English DT Article DE Mars; Radar observations; Ionospheres ID SOLAR-WIND INTERACTION; SUBSURFACE; REFLECTOMETER; IONOSPHERE; SOUNDINGS; LOWLANDS; DEPOSITS AB The MARSIS radar experiment aboard the ESA Mars Express satellite has recorded several unusual reflections in the Ma'adim Vallis region of Mars. These reflections display a wide variety of morphologies which are very different from those of reflections seen beneath the Polar Layered Deposits. Medusae Fossae Formation and Dorsa Argentea Formation. Their morphologies are sometimes very laterally extensive, parabolic or hyperbolic, and apparently deep, but they can also appear horizontal and shallow. Aided by a geological map of the Ma'adim Vallis region, the morphological, locational and temporal characteristics of the reflections have been studied individually in an attempt to constrain their origin. While some may be subsurface reflections based on their shallow morphologies and correlation with the Eridania Planitia basin network, all of the reflections are ambiguous to some degree, displaying characteristics that do not allow a definite subsurface- or possibly ionospheric-sourced mechanism to be proposed for their creation. Those with more exaggerated morphologies are regarded as being much more likely to result from ionospheric distortion rather than subsurface inhomogeneity. (C) 2009 Elsevier Inc. All rights reserved. C1 [White, Oliver L.; Stofan, Ellen R.] UCL, Birkbeck Res Sch Earth Sci, London WC1E 6BT, England. [Safaeinili, Ali; Plaut, Jeffrey J.; Heggy, Essam] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Stofan, Ellen R.] Proxemy Res, Laytonville, MD 20882 USA. [Clifford, Stephen M.] Lunar & Planetary Inst, Houston, TX 77058 USA. [Farrell, William M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Picardi, Giovanni] Univ Roma La Sapienza, Infocom Dept, I-00184 Rome, Italy. RP White, OL (reprint author), UCL, Birkbeck Res Sch Earth Sci, Gower St, London WC1E 6BT, England. EM o.white@ucl.ac.uk; ali.safaeinili@jpl.nasa.gov; plaut@mail.jpl.nasa.gov; ellen@proxemy.com; Clifford@lpi.usra.edu; William.M.Farrell@nasa.gov; essam.heggy@jpl.nasa.gov; picar@infocom.uniroma1.it RI Heggy, Essam/E-8250-2013; Farrell, William/I-4865-2013 OI Heggy, Essam/0000-0001-7476-2735; NR 30 TC 4 Z9 4 U1 1 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 JUN PY 2009 VL 201 IS 2 BP 460 EP 473 DI 10.1016/j.icarus.2009.01.015 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 446NW UT WOS:000266129300006 ER PT J AU Feaga, LM McGrath, M Feldman, PD AF Feaga, Lori M. McGrath, Melissa Feldman, Paul D. TI Io's dayside SO2 atmosphere SO ICARUS LA English DT Article DE Io; Satellites, atmospheres; Abundances, atmospheres; Hubble Space Telescope observations ID INTERPLANETARY LYMAN-ALPHA; HUBBLE-SPACE-TELESCOPE; PELE PLUME; ULTRAVIOLET SPECTROMETER; VOLCANIC ACTIVITY; SULFUR-DIOXIDE; SOLAR MAXIMUM; GALILEO; SURFACE; SPECTROSCOPY AB An extensive set of HI Lyman-alpha images obtained with the Hubble Space Telescope (HST) Space Telescope Imaging Spectrograph (STIS) from 1997-2001 has been analyzed to provide information about the spatial and temporal character of Io's SO2 atmosphere. An atmospheric distribution map derived from the observations reveals that the sunlit SO2 atmosphere is temporally stable on a global scale, with only small local changes. An anti-/sub-jovian asymmetry in the SO2 distribution is present in all 5 years of the observations. The average daytime atmosphere is densest on the anti-jovian hemisphere in the equatorial regions, with a maximum equatorial column density of 5.0 x 10(16) cm(-2) at 140 degrees longitude. The SO2 atmosphere also has greater latitudinal extent on the anti-jovian hemisphere as compared to the sub-jovian. The atmospheric distribution appears to be best correlated with the location of hot spots and known volcanic plumes, although small number statistics for the plumes limits the correlation. (C) 2009 Elsevier Inc. All rights reserved. C1 [Feaga, Lori M.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [McGrath, Melissa] NASA MSFC, Huntsville, AL 35824 USA. [Feldman, Paul D.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. RP Feaga, LM (reprint author), Univ Maryland, Dept Astron, College Pk, MD 20742 USA. EM feaga@astro.umd.edu; Melissa.A.McGrath@nasa.gov; pdf@pha.jhu.edu FU NASA [HST-AR-10313.02-A]; Association of Universities for Research in Astronomy, Incorporated, under NASA [NAS5-26555] FX Support for this work was provided by NASA through grant number HST-AR-10313.02-A from the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Incorporated, under NASA contract NAS5-26555. We would like to thank our referees for their constructive suggestions and discussion which have improved the scientific value of our paper. NR 48 TC 26 Z9 26 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 EI 1090-2643 J9 ICARUS JI Icarus PD JUN PY 2009 VL 201 IS 2 BP 570 EP 584 DI 10.1016/j.icarus.2009.01.029 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 446NW UT WOS:000266129300015 ER PT J AU Palguta, J Schubert, G Zhang, KK Anderson, JD AF Palguta, Jennifer Schubert, Gerald Zhang, Keke Anderson, John D. TI Constraints on the location, magnitude, and dimensions of Ganymede's mass anomalies SO ICARUS LA English DT Article DE Ganymede; Jupiter, satellites; Satellites, surfaces ID WATER VOLCANISM; GROOVED TERRAIN; HIGH-RESOLUTION; BRIGHT AB Previously, radio Doppler data, generated with NASA's Galileo spacecraft during its second encounter with Jupiter's moon Ganymede, were used to infer the locations and magnitudes of mass anomalies on Ganymede using point-mass models. However, the point-mass solutions do not provide the vertical and horizontal extent of the anomalous mass concentrations. Here, we provide the results of a new study using spherical cap disks to model Ganymede's mass anomalies. The spherical cap disk models not only provide the locations and magnitudes of the mass anomalies, but also their vertical and horizontal dimensions. The new models show that three disks, a positive mass located at (53.0 degrees N, 127.0 degrees W) and two negative masses located at (22.0 degrees N, 87.0 degrees W) and (49.0 degrees N, 219.0 degrees W), can explain the data. The magnitudes of the mass anomalies are on the order of 10(18) kg. The diameters of the anomalies are a few thousand kilometers. The positive anomaly is about 100 meters thick and both negative anomalies have a thickness of less than a kilometer. We use the additional information provided by the disk models to investigate the viability of mass anomalies at Ganymede's surface by comparing the diameters of the anomalies to the sizes of regiones and sulci and the anomalies' thicknesses to accumulated layers of rock and clean ice on the surface. We find that the dimensions of the mass anomalies could be explained by concentrations of rock in the regio and rock-free ice in the sulci. These results confirm that mass anomalies may reside on or near Ganymede's surface and that positive mass anomalies are contained within areas of dark terrain and negative mass anomalies within bright terrain. (C) 2009 Elsevier Inc. All rights reserved. C1 [Palguta, Jennifer; Schubert, Gerald] Univ Calif Los Angeles, Dept Earth & Space Sci, Los Angeles, CA 90095 USA. [Schubert, Gerald] Univ Calif Los Angeles, Inst Geophys & Planetary Phys, Los Angeles, CA 90095 USA. [Zhang, Keke] Univ Exeter, Dept Math Sci, Exeter EX4 4QE, Devon, England. [Anderson, John D.] Jet Prop Lab, Pasadena, CA 91106 USA. RP Palguta, J (reprint author), Univ Calif Los Angeles, Dept Earth & Space Sci, 3806 Geol, Los Angeles, CA 90095 USA. EM jpalguta@ucla.edu NR 13 TC 3 Z9 3 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 JUN PY 2009 VL 201 IS 2 BP 615 EP 625 DI 10.1016/j.icarus.2009.02.004 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 446NW UT WOS:000266129300018 ER PT J AU Meech, KJ Pittichova, J Bar-Nun, A Notesco, G Laufer, D Hainaut, OR Lowry, SC Yeomans, DK Pitts, M AF Meech, K. J. Pittichova, J. Bar-Nun, A. Notesco, G. Laufer, D. Hainaut, O. R. Lowry, S. C. Yeomans, D. K. Pitts, M. TI Activity of comets at large heliocentric distances pre-perihelion SO ICARUS LA English DT Article DE Ices; Comets, composition; Comets, origin; Photometry ID AMORPHOUS WATER ICE; SOLAR-SYSTEM; BOWELL 1980B; KUIPER-BELT; PERIOD COMETS; LONG-PERIOD; DEEP-IMPACT; OORT CLOUD; HALE-BOPP; OBJECT AB We present observational data for two long-period and three dynamically new comets observed at heliocentric distances between 5.8 to 14.0 AU. All of the comets exhibited activity beyond the distance at which water ice sublimation can be significant. We have conducted experiments on gas-laden amorphous ice samples and show that considerable gas emission occurs when the ice is heated below the temperature of the amorphous-crystalline ice phase transition (T similar to 137 K). We propose that annealing of amorphous water ice is the driver of activity in comets as they first enter the inner Solar System. Experimental data show that large grains can be ejected at low velocity during annealing and that the rate of brightening of the comet should decrease as the heliocentric distance decreases. These results are consistent with both historical observations of distant comet activity and with the data presented here. If observations of the onset of activity in a dynamically new comet are ever made, the distance at which this occurs would be a sensitive indicator of the temperature at which the comet had formed or represents the maximum temperature that it has experienced. New surveys such as Pan STARRS, may be able to detect these comets while they are still inactive. (C) 2009 Elsevier Inc. All rights reserved. C1 [Meech, K. J.; Pittichova, J.; Pitts, M.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. [Bar-Nun, A.; Notesco, G.; Laufer, D.] Tel Aviv Univ, Dept Geophys & Planetary Sci, IL-69978 Tel Aviv, Israel. [Lowry, S. C.; Yeomans, D. K.] Jet Prop Lab, Pasadena, CA 91109 USA. RP Meech, KJ (reprint author), NASA, Astrobiol Inst, Washington, DC 20546 USA. EM meech@ifa.hawaii.edu FU National Aeronautics and Space Administration through the NASA Astrobiology Institute [NNA04CC08A]; NASA [NNX07A044G]; Israel Ministry of Science, through the Israel Space Agency; Scientific Grant Agency VEGA of the Slovak Academy of Science [2/7040/27] FX This material is based upon work supported by the National Aeronautics and Space Administration through the NASA Astrobiology Institute under Cooperative Agreement No. NNA04CC08A issued through the Office of Space Science, by NASA Grant No. NNX07A044G, and through the US-Israel Bi-national foundation (BSF) and by the Israel Ministry of Science, through the Israel Space Agency. JP was supported, in part, by the Scientific Grant Agency VEGA of the Slovak Academy of Science, 2/7040/27. Image processing in this paper has been performed using the IRAF software. IRAF is distributed by the National Optical Astronomy Observatories, which is operated by the Association of Universities for Research in Astronomy, Inc. (AURA) under cooperative agreement with the National Science Foundation. We thank A. Fitz Simmons and an anonymous referee for their helpful comments on the manuscript. NR 77 TC 41 Z9 41 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 JUN PY 2009 VL 201 IS 2 BP 719 EP 739 DI 10.1016/j.icarus.2008.12.045 PG 21 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 446NW UT WOS:000266129300025 ER PT J AU Pompilio, L Pedrazzi, G Sgavetti, M Cloutis, EA Craig, MA Roush, TL AF Pompilio, Loredana Pedrazzi, Giuseppe Sgavetti, Maria Cloutis, Edward A. Craig, Michael A. Roush, Ted L. TI Exponential Gaussian approach for spectral modeling: The EGO algorithm I. Band saturation SO ICARUS LA English DT Article DE Spectroscopy; Mineralogy ID REFLECTANCE SPECTRA; MARTIAN METEORITES; PYROXENE MIXTURES; ABSORPTION-BANDS; SPECTROSCOPY; OLIVINE; MINERALS; REGION; IRON AB Curve fitting techniques are a widespread approach to spectral modeling in the VNIR range [Burns, R.G., 1970. Am. Mineral. 55, 1608-1632; Singer, R.B., 1981. J. Geophys. Res. 86, 7967-7982; Roush, T.L., Singer, R.B., 1986. J. Geophys. Res. 91, 10301-10308; Sunshine, J.M., Pieters, C.M., Pratt, S.F., 1990. J. Geophys. Res. 95, 6955-6966]. They have been successfully used to model reflectance spectra of powdered minerals and mixtures, natural rock samples and meteorites, and unknown remote spectra of the Moon, Mars and asteroids. Here, we test a new decomposition algorithm to model VNIR reflectance spectra and call it Exponential Gaussian Optimization (EGO). The EGO algorithm is derived from and complementary to the MGM of Sunshine et al. [Sunshine, J.M., Pieters, C.M., Pratt, S.F., 1990. J. Geophys. Res. 95, 6955-6966]. The general EGO equation has been especially designed to account for absorption bands affected by saturation and asymmetry. Here we present a special case of EGO and address it to model saturated electronic transition bands. Our main goals are: (1) to recognize and model band saturation in reflectance spectra; (2) to develop a basic approach for decomposition of rock spectra, where effects due to saturation are most prevalent; (3) to reduce the uncertainty related to quantitative estimation when band saturation is occurring. In order to accomplish these objectives, we simulate flat bands starting from pure Gaussians and test the EGO algorithm on those Simulated spectra first. Then we test the EGO algorithm on a number of measurements acquired on powdered pyroxenes having different compositions and average grain size and binary mixtures of orthopyroxenes with barium sulfate. The main results arising from this study are: (1) EGO model is able to numerically account for the occurrence of saturation effects on reflectance spectra of powdered minerals and mixtures; (2) the systematic dilution of a strong absorber using a bright neutral material is not responsible for band deformation. Further work is still required in order to analyze the behavior of the EGO algorithm with respect to the saturation phenomena using more complex band shapes than pyroxene bands. (C) 2009 Elsevier Inc. All rights reserved. C1 [Pompilio, Loredana; Sgavetti, Maria] Univ Parma, Dipartimento Sci Terra, I-43100 Parma, Italy. [Pedrazzi, Giuseppe] Univ Parma, Dipartimento Sanita Pubbl, Sez Fis, I-43100 Parma, Italy. [Cloutis, Edward A.; Craig, Michael A.] Univ Winnipeg, Dept Geog, Winnipeg, MB R3B 2E9, Canada. [Roush, Ted L.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Pompilio, L (reprint author), Univ Parma, Dipartimento Sci Terra, Via Usberti 157A, I-43100 Parma, Italy. EM loredana.pompilio@unipr.it OI Pedrazzi, Giuseppe/0000-0002-5971-2040 NR 45 TC 13 Z9 13 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 JUN PY 2009 VL 201 IS 2 BP 781 EP 794 DI 10.1016/j.icarus.2009.01.022 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 446NW UT WOS:000266129300029 ER PT J AU Wilson, CF Tsang, CCC Irwin, PGJ Taylor, FW Bezard, B Erard, S Carlson, RW Drossart, P Piccioni, G Holmes, RC AF Wilson, C. F. Tsang, C. C. C. Irwin, P. G. J. Taylor, F. W. Bezard, B. Erard, S. Carlson, R. W. Drossart, P. Piccioni, G. Holmes, R. C. TI Analysis of thermal emission from the nightside of Venus at 1.51 and 1.55 mu m SO ICARUS LA English DT Article DE Venus; Infrared observations; Radiative transfer; Venus Express ID RADIATIVE-TRANSFER; DARK SIDE; ATMOSPHERE; SPECTRA; SURFACE AB We present radiative transfer modelling of thermal emission from the nightside of Venus in two 'spectral window' regions at 1.51 and 1.55 mu m. The first discovery of these windows, reported by Erard et al. [Erard. S., Drossart, P., Piccioni, G., 2009. J. Geophys. Res. Planets 114, doi:10.1029/2008JE003116. E00B27], was achieved using a principal component analysis of data from the VIRTIS instrument on Venus Express. These windows are spectrally narrow, with a full-width at half-maximum of similar to 20 nm, and less bright than the well-known 1.7 and 2.3 mu m spectral windows by two orders of magnitude. In this note we present the first radiative transfer analysis of these windows. We conclude that the radiation in these windows originates at an altitude of 20-35 km. As is the case for the other infrared window regions, the brightness of the windows is affected primarily by the optical depth of the overlying clouds; in addition, the 1.51 mu m radiance shows a very weak sensitivity to water vapour abundance. (C) 2009 Elsevier Inc. All rights reserved. C1 [Wilson, C. F.; Tsang, C. C. C.; Irwin, P. G. J.; Taylor, F. W.; Holmes, R. C.] Univ Oxford, Dept Phys, AOPP, Oxford OX1 3PU, England. [Bezard, B.; Erard, S.; Drossart, P.] Observ Paris, CNRS, LESIA, UMR 8109, F-92195 Meudon, France. [Carlson, R. W.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Piccioni, G.] INAF IASF, I-00133 Rome, Italy. RP Wilson, CF (reprint author), Univ Oxford, Dept Phys, AOPP, Oxford OX1 3PU, England. EM wilson@atm.ox.ac.uk FU STFC; ASI; CNES; NASA FX We acknowledge the entire Venus Express and VIRTIS teams, as well as funding from national agencies STFC, ASI, CNES and NASA. NR 22 TC 3 Z9 3 U1 0 U2 1 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 JUN PY 2009 VL 201 IS 2 BP 814 EP 817 DI 10.1016/j.icarus.2009.03.010 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 446NW UT WOS:000266129300032 ER PT J AU Leong, KMKH Deal, WR Radisic, V Mei, XB Uyeda, J Samoska, L Fung, A Gaier, T Lai, R AF Leong, Kevin M. K. H. Deal, William R. Radisic, Vesna Mei, Xiao Bing Uyeda, Jansen Samoska, Lorene Fung, Andy Gaier, Todd Lai, Richard TI A 340-380 GHz Integrated CB-CPW-to-Waveguide Transition for Sub Millimeter-Wave MMIC Packaging SO IEEE MICROWAVE AND WIRELESS COMPONENTS LETTERS LA English DT Article DE Coplanar waveguide (CPW); monolithic microwave integrated circuit (MMIC); waveguide transition AB In this letter, a rectangular waveguide to conductor backed-coplanar waveguide electromagnetic transition suitable of operating at sub-millimeter wave frequencies is demonstrated. The dipole based transition is fabricated using InP monolithic microwave integrated circuit technology. The compact transition eliminates wire-bonding problems (return loss and insertion loss) and is suitable for direct integration of sub-millimeter wave monolithic integrated circuits. Measured transition loss of similar to 1 dB has been achieved in the frequency range of 340 to 380 GHz. C1 [Leong, Kevin M. K. H.; Deal, William R.; Radisic, Vesna; Mei, Xiao Bing; Uyeda, Jansen; Lai, Richard] Northrop Grumman Corp, Redondo Beach, CA 90278 USA. [Samoska, Lorene; Fung, Andy; Gaier, Todd] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Leong, KMKH (reprint author), Northrop Grumman Corp, Redondo Beach, CA 90278 USA. EM kevin.leong@ngc.com FU DARPA SWIFT Program; Army Research Laboratory [W911QX-06-C-0050] FX Manuscript received January 08, 2009; revised January 27, 2009. First published May 26, 2009; current version published June 05, 2009. This work was supported by the DARPA SWIFT Program and Army Research Laboratory under ARL Contract W911QX-06-C-0050. NR 9 TC 27 Z9 27 U1 0 U2 4 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 JUN PY 2009 VL 19 IS 6 BP 413 EP 415 DI 10.1109/LMWC.2009.2020043 PG 3 WC Engineering, Electrical & Electronic SC Engineering GA 464HP UT WOS:000267496300025 ER PT J AU Kerber, GL Kleinsasser, AW Bumble, B AF Kerber, G. L. Kleinsasser, A. W. Bumble, B. TI Fabrication of Submicrometer High Current Density Nb/Al-AlNx/Nb Junctions SO IEEE TRANSACTIONS ON APPLIED SUPERCONDUCTIVITY LA English DT Article; Proceedings Paper CT Applied Superconductivity Conference CY AUG 17-22, 2008 CL Chicago, IL SP ATI Wah Chang, Coalit Commercial Applicat Superconductors, CryoZone, GE Global Res Ctr, IEEE Council Superconductiv, IEEE Magnet Soc, PHPK Technologies, SuperPower Inc, Teax Ctr Superconductiv, Univ Houston DE Aluminum nitride; critical current spreads; deep-UV lithography; ICP; inductively coupled plasma; Josephson junction; niobium; rapid single flux quantum; RSFQ; self-aligned; superconductor integrated circuit fabrication ID ANODIZATION PROCESS; TUNNEL-JUNCTIONS; JOSEPHSON; FREQUENCY; CIRCUIT; MIXER; GHZ AB We have developed a sub-mu m Nb/Al-AlNx/Nb Josephson junction and integrated circuit fabrication process using deep-UV lithography and inductively coupled plasma etch tools. The baseline process consists of 11 masking steps including ground plane, PdAu resistor, Nb/Al-AlNx/Nb trilayer, and two additional Nb wiring layers. The AlNx tunnel barriers are grown with plasma nitridation. These junctions exhibit low subgap leakage even at current densities exceeding 100 kA/cm(2). The critical current spread of a series array of 50-kA/cm(2), 0.6 mu m diameter junctions is under 3%. For very high current density applications, these junctions are a good candidate to replace Nb/Al-AlOx/Nb junctions particularly in future generations of very high speed, rapid single flux quantum logic circuits. In this paper we discuss our baseline fabrication process and device characterization including junction capacitance extraction from direct measurements of the Josephson plasma frequency. C1 [Kerber, G. L.; Kleinsasser, A. W.; Bumble, B.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Kerber, GL (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM george.l.kerber@jpl.nasa.gov; alan.w.kleinsasser@jpl.nasa.gov; b.bumble@jpl.nasa.gov NR 19 TC 5 Z9 5 U1 0 U2 16 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 1051-8223 J9 IEEE T APPL SUPERCON JI IEEE Trans. Appl. Supercond. PD JUN PY 2009 VL 19 IS 3 BP 159 EP 166 DI 10.1109/TASC.2009.2017859 PN 1 PG 8 WC Engineering, Electrical & Electronic; Physics, Applied SC Engineering; Physics GA 474KK UT WOS:000268282000009 ER PT J AU Bumble, B Fung, A Kaul, AB Kleinsasser, AW Kerber, GL Bunyk, P Ladizinsky, E AF Bumble, Bruce Fung, Andy Kaul, Anu B. Kleinsasser, Alan W. Kerber, George L. Bunyk, Paul Ladizinsky, Eric TI Submicrometer Nb/Al-AlOx/Nb Integrated Circuit Fabrication Process for Quantum Computing Applications SO IEEE TRANSACTIONS ON APPLIED SUPERCONDUCTIVITY LA English DT Article; Proceedings Paper CT Applied Superconductivity Conference CY AUG 17-22, 2008 CL Chicago, IL SP ATI Wah Chang, Coalit Commercial Applicat Superconductors, CryoZone, GE Global Res Ctr, IEEE Council Superconductiv, IEEE Magnet Soc, PHPK Technologies, SuperPower Inc, Teax Ctr Superconductiv, Univ Houston DE Quantum computing; SQUIDs; superconducting devices AB We have developed a low J(c) (100-1000 A/cm(2)) submicrometer Nb integrated circuit fabrication process for SQUID-ased quantum computing applications. The baseline process consists of 7 masking steps including Pd-Au resistor, Nb/Al-AlOx/Nb trilayer, two Nb wiring layers and two sputtered SiO2 dielectric layers. We have also fabricated wafers with an Nb ground plane. Using deep-UV lithography, inductively coupled plasma etch tools, and self-aligned lift-off for device definition, we routinely achieve micrometer lines and spaces with 400 nm minimum junction dimensions. Room temperature testing is used to select wafers in process and junction annealing has been calibrated for trimming current density. We will describe the process which has been used to produce circuits with over 100 junctions. C1 [Bumble, Bruce; Fung, Andy; Kaul, Anu B.; Kleinsasser, Alan W.; Kerber, George L.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Bunyk, Paul; Ladizinsky, Eric] D Wave Syst Inc, Vancouver, BC, Canada. RP Bumble, B (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM Bruce.Bumble@jpl.nasa.gov; kingman.fung@jpl.nasa.gov; Anu.b.kaul@jpl.nasa.gov; Alan.Kleinsasser@jpl.nasa.gov; George.L.Kerber@jpl.nasa.gov; pbunyk@dwavesys.com; Eric@dwavesys.com NR 11 TC 3 Z9 3 U1 0 U2 1 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 1051-8223 J9 IEEE T APPL SUPERCON JI IEEE Trans. Appl. Supercond. PD JUN PY 2009 VL 19 IS 3 BP 226 EP 229 DI 10.1109/TASC.2009.2018249 PN 1 PG 4 WC Engineering, Electrical & Electronic; Physics, Applied SC Engineering; Physics GA 474KK UT WOS:000268282000024 ER PT J AU Aslam, S Stevenson, TR Hsieh, WT Travers, DE Jones, HH Lakew, B AF Aslam, Shahid Stevenson, Thomas R. Hsieh, Wen-Ting Travers, Douglas E. Jones, Hollis H. Lakew, Brook TI Etching of MgB2 Thin Films for Transition Edge Superconducting Bolometer Fabrication SO IEEE TRANSACTIONS ON APPLIED SUPERCONDUCTIVITY LA English DT Article; Proceedings Paper CT Applied Superconductivity Conference CY AUG 17-22, 2008 CL Chicago, IL SP ATI Wah Chang, Coalit Commercial Applicat Superconductors, CryoZone, GE Global Res Ctr, IEEE Council Superconductiv, IEEE Magnet Soc, PHPK Technologies, SuperPower Inc, Teax Ctr Superconductiv, Univ Houston DE Bolometer; Cl-plasma based etch; etching; HCl-etch; HNO3-etch; MgB2; superconducting transition; thin film AB Membrane-structured superconducting MgB2 thin films are potential candidates for the development of moderately cooled bolometers sensitive to far infra-red radiation. On the path to developing such devices, we present a comparison of three etching techniques for MgB2 thin films namely, chlorine plasma etch, aqueous hydrochloric acid etch and an aqueous nitric acid etch. Out of the three etch techniques, the aqueous 50% nitric acid solution etch, using standard photolithography, proved to have a high MgB2 etch rate (> 51 nm/s), with better sidewall delineation and selectivity to the underlying SiN-film-coated Si substrate, moreover the etched film structure showed good superconductivity transition characteristics, namely, a superconducting critical transition at 38.57 +/- 0.6 K, a transition width of 0.09 K and a of 2.22. C1 [Aslam, Shahid; Travers, Douglas E.] MEI Technol Inc, Houston, TX 77058 USA. [Stevenson, Thomas R.; Hsieh, Wen-Ting; Jones, Hollis H.; Lakew, Brook] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Aslam, S (reprint author), MEI Technol Inc, Houston, TX 77058 USA. EM shahid.aslam-1@nasa.gov; thomas.r.stevenson@nasa.gov; wen-ting.hsieh-1@nasal.gov; douglas.e.travers@nasa.gov; hollis.h.jones@nasa.gov; brook.lakew-1@nasa.gov RI Aslam, Shahid/D-1099-2012 NR 19 TC 2 Z9 2 U1 1 U2 7 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 1051-8223 J9 IEEE T APPL SUPERCON JI IEEE Trans. Appl. Supercond. PD JUN PY 2009 VL 19 IS 3 BP 257 EP 260 DI 10.1109/TASC.2009.2017855 PN 1 PG 4 WC Engineering, Electrical & Electronic; Physics, Applied SC Engineering; Physics GA 474KK UT WOS:000268282000032 ER PT J AU Karpov, A Miller, D Stern, JA Bumble, B LeDuc, HG Zmuidzinas, J AF Karpov, A. Miller, D. Stern, J. A. Bumble, B. LeDuc, H. G. Zmuidzinas, J. TI Development of Low Noise THz SIS Mixer Using an Array of Nb/Al-AlN/NbTiN Junctions SO IEEE TRANSACTIONS ON APPLIED SUPERCONDUCTIVITY LA English DT Article; Proceedings Paper CT Applied Superconductivity Conference CY AUG 17-22, 2008 CL Chicago, IL SP ATI Wah Chang, Coalit Commercial Applicat Superconductors, CryoZone, GE Global Res Ctr, IEEE Council Superconductiv, IEEE Magnet Soc, PHPK Technologies, SuperPower Inc, Teax Ctr Superconductiv, Univ Houston DE Niobium alloys; radio astronomy; submillimeter wave receivers; superconductor-insulator-superconductor mixers; THz technology ID MILLIMETER; ASTRONOMY; RECEIVERS; SOFIA AB We report the development of a low noise and broadband SIS mixer aimed for 1 THz channel of the Caltech Airborne Submillimeter Interstellar Medium Investigations Receiver (CASIMIR), designed for the Stratospheric Observatory for Infrared Astronomy, (SOFIA). The mixer uses an array of two 0.24 mu m(2) Nb/Al-AlN/NbTiN SIS junctions with the critical current density of 30-50 kA/cm(2). An on-chip double slot planar antenna couples the mixer circuit with the telescope beam. The mixer matching circuit is made with Nb and gold films. The mixer IF circuit is designed to cover 4-8 GHz band. A test receiver with the new mixer has a low noise operation in 0.87-1.12 THz band. The minimum receiver noise measured in our experiment is 353 K (Y = 1.50). The receiver noise corrected for the loss in the LO injection beam splitter is 250 K. The combination of a broad operation band of about 250 GHz with a low receiver noise makes the new mixer a useful element for application at SOFIA. C1 [Karpov, A.; Miller, D.; Zmuidzinas, J.] CALTECH, Dept Phys, Pasadena, CA 91125 USA. [Stern, J. A.; Bumble, B.; LeDuc, H. G.] CALTECH, Jet Prop Lab, MDL, Pasadena, CA 91109 USA. RP Karpov, A (reprint author), CALTECH, Dept Phys, Pasadena, CA 91125 USA. EM karpov@submm.caleh.edu NR 15 TC 1 Z9 1 U1 2 U2 9 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855 USA SN 1051-8223 J9 IEEE T APPL SUPERCON JI IEEE Trans. Appl. Supercond. PD JUN PY 2009 VL 19 IS 3 BP 305 EP 308 DI 10.1109/TASC.2009.2017913 PG 4 WC Engineering, Electrical & Electronic; Physics, Applied SC Engineering; Physics GA 474KK UT WOS:000268282000043 ER PT J AU Smith, SJ Bandler, SR Brekosky, RP Brown, AD Chervenak, JA Eckart, ME Figueroa-Feliciano, E Finkbeiner, FM Kelley, RL Kilbourne, CA Porter, FS Sadleir, JE AF Smith, Stephen James Bandler, Simon R. Brekosky, Regis P. Brown, Ari-David Chervenak, Jay A. Eckart, Megan E. Figueroa-Feliciano, Encetali Finkbeiner, Fred M. Kelley, Richard L. Kilbourne, Caroline A. Porter, Frederick Scott Sadleir, John E. TI Development of Position-Sensitive Transition-Edge Sensor X-Ray Detectors SO IEEE TRANSACTIONS ON APPLIED SUPERCONDUCTIVITY LA English DT Article; Proceedings Paper CT Applied Superconductivity Conference CY AUG 17-22, 2008 CL Chicago, IL SP ATI Wah Chang, Coalit Commercial Applicat Superconductors, CryoZone, GE Global Res Ctr, IEEE Council Superconductiv, IEEE Magnet Soc, PHPK Technologies, SuperPower Inc, Teax Ctr Superconductiv, Univ Houston DE Hydra; microcalorimeter; position-sensitive detector; transition-edge sensor ID MICROCALORIMETERS AB We report on the development of position- sensitive transition-edge sensors (PoST's) for future X-ray astronomy missions such as the International X-ray Observatory (IXO), under study by NASA and ESA. PoST's consist of multiple absorbers each with a different thermal coupling to one or more transition-edge sensors (TESs). This results in a characteristic pulse shape for each absorber element and allows position discrimination. PoST development is motivated by a desire to achieve maximum focal-plane area with the fewest number of readout channels. We report detailed characterization of our single TES PoST's or Hydras, which consist of four electroplated Au/Bi absorbers coupled to a low noise Mo/Au TES. Using a numerical model of the Hydra we fit to measured complex impedance curves and determine device parameters that allow us to accurately reproduce the measured pulse shapes and noise spectra. Results from Hydras with different internal thermal conductances reveal the trade-offs in optimizing for energy resolution or position- sensitivity. We report a best achievable energy resolution of 6.0 eV across all pixels for a device with transition temperature of 86 mK, coupled with straightforward position discrimination by rise-time. C1 [Smith, Stephen James; Bandler, Simon R.; Brekosky, Regis P.; Brown, Ari-David; Chervenak, Jay A.; Eckart, Megan E.; Finkbeiner, Fred M.; Kelley, Richard L.; Kilbourne, Caroline A.; Porter, Frederick Scott; Sadleir, John E.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Bandler, Simon R.] Univ Maryland, College Pk, MD 20742 USA. [Brekosky, Regis P.] Northrop Grumman Corp, Lanham, MD 20706 USA. [Figueroa-Feliciano, Encetali] MIT, Cambridge, MA 02139 USA. [Finkbeiner, Fred M.] Wyle Informat Syst, Mclean, VA 22102 USA. [Sadleir, John E.] Univ Illinois, Urbana, IL 61801 USA. RP Smith, SJ (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. EM stephen.j.smith@nasa.gov; Simon.R.Bandler@nasa.gov; Regis.P.Brekosky@nasa.gov; ari.d.brown@nasa.gov; James.A.Chervenak@nasa.gov; Megan.E.Eckart@nasa.gov; enectali@MIT.EDU; Fred.M.Finkbeiner@nasa.gov; Richard.L.Kelley@nasa.gov; Caroline.A.Kilbourne@nasa.gov; Fred-erick.S.Porter@nasa.gov; john.e.sadleir@nasa.gov 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 17 TC 11 Z9 11 U1 2 U2 9 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855 USA SN 1051-8223 J9 IEEE T APPL SUPERCON JI IEEE Trans. Appl. Supercond. PD JUN PY 2009 VL 19 IS 3 BP 451 EP 455 DI 10.1109/TASC.2009.2019557 PG 5 WC Engineering, Electrical & Electronic; Physics, Applied SC Engineering; Physics GA 474KK UT WOS:000268282000075 ER PT J AU Beyer, J Drung, D Peters, M Schurig, T Bandler, SR AF Beyer, Joern Drung, Dietmar Peters, Margret Schurig, Thomas Bandler, Simon R. TI A Single-Stage SQUID Multiplexer for TES Array Readout SO IEEE TRANSACTIONS ON APPLIED SUPERCONDUCTIVITY LA English DT Article; Proceedings Paper CT Applied Superconductivity Conference CY AUG 17-22, 2008 CL Chicago, IL SP ATI Wah Chang, Coalit Commercial Applicat Superconductors, CryoZone, GE Global Res Ctr, IEEE Council Superconductiv, IEEE Magnet Soc, PHPK Technologies, SuperPower Inc, Teax Ctr Superconductiv, Univ Houston DE SQUID multiplexers; SQUID series arrays; transition edge sensors ID TRANSITION-EDGE SENSORS AB We have developed a single-stage SQUID multiplexer (SQMUX) for time-domain multiplexing of transition edge sensors (TESs). The individual channels in our SQMUX circuit are SQUID series arrays (SSAs). Several of these SSAs form one column, of which exactly one SSA is active at a time. The channel to be read out is selected by setting a superconducting-to-normal conducting (SN) switch into its normalconducting state. All other channels are short-circuited by SN-switches in their superconducting state. This SQMUX topology ensures that there are no noise contributions from off-channels. The SN-switches employed are SSAs, as well. The addressing is performed inductively by means of coupling magnetic flux into the switch. Our SQMUX can be operated at the TES operating temperature. It is directly read out by a room temperature preamplifier. The first realizations of this single-stage SQMUX are 4:1 and 2:2 multiplexers. We present the application of the new SQMUX to read out TES X-ray microcalorimeters. Furthermore, we discuss the application of SQMUXs to the readout of Distributed Power TES Detectors. C1 [Beyer, Joern; Drung, Dietmar; Peters, Margret; Schurig, Thomas] Phys Tech Bundesanstalt Berlin, D-10587 Berlin, Germany. [Bandler, Simon R.] Univ Maryland, College Pk, MD 20742 USA. [Bandler, Simon R.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Bandler, Simon R.] CRESST, College Pk, MD 20742 USA. RP Beyer, J (reprint author), Phys Tech Bundesanstalt Berlin, D-10587 Berlin, Germany. EM joern.beyer@ptb.de; dietmar.drung@ptb.de; margret.peters@ptb.de; thomas.schurig@ptb.de; Simon.R.Bandler@nasa.gov RI Bandler, Simon/A-6258-2010 OI Bandler, Simon/0000-0002-5112-8106 NR 14 TC 2 Z9 2 U1 1 U2 5 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 1051-8223 EI 1558-2515 J9 IEEE T APPL SUPERCON JI IEEE Trans. Appl. Supercond. PD JUN PY 2009 VL 19 IS 3 BP 505 EP 508 DI 10.1109/TASC.2009.2018195 PN 1 PG 4 WC Engineering, Electrical & Electronic; Physics, Applied SC Engineering; Physics GA 474KK UT WOS:000268282000088 ER PT J AU Bonetti, JA Day, PK Kenyon, M Kuo, CL Turner, A LeDuc, HG Bock, JJ AF Bonetti, Joseph A. Day, Peter K. Kenyon, Matthew Kuo, Chao-Lin Turner, Anthony LeDuc, H. G. Bock, James J. TI Characterization of Antenna-Coupled TES Bolometers for the Spider Experiment SO IEEE TRANSACTIONS ON APPLIED SUPERCONDUCTIVITY LA English DT Article; Proceedings Paper CT Applied Superconductivity Conference CY AUG 17-22, 2008 CL Chicago, IL SP ATI Wah Chang, Coalit Commercial Applicat Superconductors, CryoZone, GE Global Res Ctr, IEEE Council Superconductiv, IEEE Magnet Soc, PHPK Technologies, SuperPower Inc, Teax Ctr Superconductiv, Univ Houston DE CMB; cosmic microwave background; polarization; TES bolometers ID ELECTROTHERMAL FEEDBACK AB We describe the transition-edge-sensors (TES's) to be employed on the Spider experiment, a balloon-based observatory whose goal is detecting the imprint of gravitational waves by mapping the polarization of the cosmic microwave background (CMB). The devices consist of Ti and Al thermistors in series sitting on a thermally isolated suspended membrane. Also on the membrane is a termination resistor coupled through a superconducting microstrip line to an on-chip, polarization sensitive, 150 GHz slot-array antenna. Several important parameters were measured. Transition temperatures were deduced by measuring the Johnson noise in the Ti thermistor. The thermal conductance between the isolated TES islands and substrate was measured by obtaining current-voltage measurements at various temperatures. The Electrical noise equivalent power was measured to sub-Hertz frequencies with varying sample geometries including those with and without normal metal bars (zebra stripes). Finally, the time constant of the devices was measured within the Al and Ti transitions where electrothermal feedback speeds up the bolometer response. This time response is 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, Joseph A.; Day, Peter K.; Kenyon, Matthew; Turner, Anthony; LeDuc, H. G.; Bock, James J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Kuo, Chao-Lin] Stanford Univ, Dept Phys, Stanford, CA 94305 USA. RP Bonetti, JA (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM joseph.bonetti@jpl.nasa.gov; clkuo@stanford.edu NR 3 TC 2 Z9 2 U1 1 U2 7 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855 USA SN 1051-8223 J9 IEEE T APPL SUPERCON JI IEEE Trans. Appl. Supercond. PD JUN PY 2009 VL 19 IS 3 BP 520 EP 523 DI 10.1109/TASC.2009.2019297 PG 4 WC Engineering, Electrical & Electronic; Physics, Applied SC Engineering; Physics GA 474KK UT WOS:000268282000092 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 Heat Capacity of Absorbers for Transition-Edge Sensors Suitable for Space-Borne Far-IR/Submm Spectroscopy SO IEEE TRANSACTIONS ON APPLIED SUPERCONDUCTIVITY LA English DT Article; Proceedings Paper CT Applied Superconductivity Conference CY AUG 17-22, 2008 CL Chicago, IL SP ATI Wah Chang, Coalit Commercial Applicat Superconductors, CryoZone, GE Global Res Ctr, IEEE Council Superconductiv, IEEE Magnet Soc, PHPK Technologies, SuperPower Inc, Teax Ctr Superconductiv, Univ Houston DE Far-IR spectrometer; Si(x)N(y) heat capacity; submillimeter spectrometer; transition-edge sensor AB Using a noise thermometry technique, we measured the temperature dependence of the heat capacity C(T) of suspended Si(x)N(y) membranes for two different geometries from 30 mK to 300 mK. We determined a volumetric specific heat of the Si(x)N(y) on the order of 10 aJ/(mu m(3) K) at 0.1 K for both absorber geometries. This value for the specific heat is comparable to a typical metal and is more than a factor of 10 larger than typical glassy materials. This result affects the design of highly efficient optical absorbers for membrane-isolated transition-edge sensors (TESs) for the Background-Limited far-IR/Submillimeter Spectrograph (BLISS), a proposed grating spectrometer that could fly on the next generation of large, cryogenic space-borne telescopes. We show that it is possible to reduce the thermal mass of the absorber of TESs so the effective response time tau(e) is less than 100 ms-a requirement for all the wavelength bands for BLISS. C1 [Kenyon, M.; Day, P. K.; Bradford, C. M.; Bock, J. J.; Leduc, H. G.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Kenyon, M (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM mkenyon@jpl.nasa.gov; peter.k.day@jpl.nasa.gov; Bradford@submm.caltehc.edu; jjb@tes.cal-tech.edu; henry.g.leduc@jpl.nasa.gov NR 13 TC 3 Z9 3 U1 0 U2 3 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855 USA SN 1051-8223 J9 IEEE T APPL SUPERCON JI IEEE Trans. Appl. Supercond. PD JUN PY 2009 VL 19 IS 3 BP 524 EP 527 DI 10.1109/TASC.2009.2017703 PG 4 WC Engineering, Electrical & Electronic; Physics, Applied SC Engineering; Physics GA 474KK UT WOS:000268282000093 ER PT J AU Barrentine, EM Ali, S Allen, CA Brown, AD Cao, NT Chervenak, JA Denis, KL Hsieh, WT Miller, TM Moseley, SH Stevenson, TR Timbie, PT Travers, DE U-Yen, K Wollack, EJ AF Barrentine, Emily M. Ali, Shafinaz Allen, Christine A. Brown, Ari D. Cao, Nga T. Chervenak, James A. Denis, Kevin L. Hsieh, Wen-Ting Miller, Timothy M. Moseley, S. Harvey Stevenson, Thomas R. Timbie, Peter T. Travers, Douglas E. U-Yen, Kongpop Wollack, Edward J. TI Design of a Transition-Edge Hot-Electron Microbolometer for Millimeter-Wave Astrophysical Observations SO IEEE TRANSACTIONS ON APPLIED SUPERCONDUCTIVITY LA English DT Article; Proceedings Paper CT Applied Superconductivity Conference CY AUG 17-22, 2008 CL Chicago, IL SP ATI Wah Chang, Coalit Commercial Applicat Superconductors, CryoZone, GE Global Res Ctr, IEEE Council Superconductiv, IEEE Magnet Soc, PHPK Technologies, SuperPower Inc, Teax Ctr Superconductiv, Univ Houston DE Bolometers; hot-electron; millimeter wave detectors; superconducting sensors ID ELECTROTHERMAL FEEDBACK; BOLOMETERS AB We are developing a Transition-edge Hot-electron Microbolometer (THM) with the capacity to make sensitive and broadband astrophysical observations over frequencies ranging from 30-300 GHz (10-1 mm). This micron-sized bolometer consists of a superconducting bilayer Transition-Edge Sensor (TES) and a thin-film absorber. The THM employs the decoupling between electrons and phonons at low temperatures (below 300 mK) to provide thermal isolation. The devices are fabricated photolithographically and read out with Superconducting Quantum Interference Devices (SQUIDs). We present the details of a thermal model for a THM detector and the design for new thermally optimized antenna-coupled THMs for illumination by a RF source at 40 and 100 GHz. C1 [Barrentine, Emily M.; Timbie, Peter T.] Univ Wisconsin, Madison, WI 53706 USA. [Ali, Shafinaz] Merritt Coll, Oakland, CA 94619 USA. [Allen, Christine A.; Brown, Ari D.; Cao, Nga T.; Chervenak, James A.; Denis, Kevin L.; Hsieh, Wen-Ting; Miller, Timothy M.; Moseley, S. Harvey; Stevenson, Thomas R.; Travers, Douglas E.; U-Yen, Kongpop; Wollack, Edward J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Barrentine, EM (reprint author), Univ Wisconsin, Madison, WI 53706 USA. EM barrentine@wisc.edu RI Moseley, Harvey/D-5069-2012; Wollack, Edward/D-4467-2012 OI Wollack, Edward/0000-0002-7567-4451 NR 21 TC 0 Z9 0 U1 0 U2 2 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855 USA SN 1051-8223 J9 IEEE T APPL SUPERCON JI IEEE Trans. Appl. Supercond. PD JUN PY 2009 VL 19 IS 3 BP 528 EP 531 DI 10.1109/TASC.2009.2017956 PG 4 WC Engineering, Electrical & Electronic; Physics, Applied SC Engineering; Physics GA 474KK UT WOS:000268282000094 ER PT J AU Karasik, BS Pereverzev, SV Olaya, D Wei, J Gershenson, ME Sergeev, AV AF Karasik, Boris S. Pereverzev, Sergey V. Olaya, David Wei, Jian Gershenson, Michael E. Sergeev, Andrei V. TI Noise Measurements in Hot-Electron Titanium Nanobolometers SO IEEE TRANSACTIONS ON APPLIED SUPERCONDUCTIVITY LA English DT Article; Proceedings Paper CT Applied Superconductivity Conference CY AUG 17-22, 2008 CL Chicago, IL SP ATI Wah Chang, Coalit Commercial Applicat Superconductors, CryoZone, GE Global Res Ctr, IEEE Council Superconductiv, IEEE Magnet Soc, PHPK Technologies, SuperPower Inc, Teax Ctr Superconductiv, Univ Houston DE Bolometers; submillimeter wave detectors; superconducting device noise; superconducting radiation detectors ID RESISTIVE STATE; DIRECT DETECTOR; ASTROPHYSICS; SAFIR AB We are presenting experimental results on the electrical noise in small titanium hot-electron nanobolometers with the critical temperature above 300 mK. The noise data demonstrate good agreement with the conventional bolometer theory prediction. The noise is dominated by the thermal energy fluctuations (phonon noise) when the operating temperature is set just a few mK below the superconducting transition. The corresponding noise equivalent power (NEP) is about 3 X 10(-18) W/Hz(1/2) for the smallest measured device. The relative NEP's for the two devices measured scale roughly as the square root of the device volume as one would expect from the theory. Therefore an additional factor of 2-3 reduction of may be feasible if the length and width of our device are further reduced. The demonstrated combination of the low NEP and the relatively high operating temperature is attractive for submillimeter low-background applications. C1 [Karasik, Boris S.; Pereverzev, Sergey V.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Olaya, David; Wei, Jian; Gershenson, Michael E.] Rutgers State Univ, Piscataway, NJ 08854 USA. [Sergeev, Andrei V.] SUNY Buffalo, Buffalo, NY 14260 USA. RP Karasik, BS (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM boris.s.karasik@jpl.nasa.gov; david.olaya@nist.gov; jian-wei@northwestern.edu; gersh@physics.rutgers.edu; asergeev@eng.buffalo.edu RI Wei, Jian/B-2137-2014; Karasik, Boris/C-5918-2011 OI Wei, Jian/0000-0002-8831-6418; NR 19 TC 7 Z9 7 U1 0 U2 5 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855 USA SN 1051-8223 J9 IEEE T APPL SUPERCON JI IEEE Trans. Appl. Supercond. PD JUN PY 2009 VL 19 IS 3 BP 532 EP 535 DI 10.1109/TASC.2009.2019426 PG 4 WC Engineering, Electrical & Electronic; Physics, Applied SC Engineering; Physics GA 474KK UT WOS:000268282000095 ER PT J AU Wikus, P Rutherford, JM Adams, JS Bagdasarova, Y Bandler, SR Bautz, M Boyce, K Brown, G Deiker, S Doriese, WB Figueroa-Feliciano, E Flanagan, K Galeazzi, M Hilton, GC Hwang, U Irwin, KD Kelley, RL Kallman, T Kilbourne, CA Kissel, S Leman, SW Levine, A Loewenstein, M Martinez-Galarce, D Mushotzky, R McCammon, D Najjar, D Petre, R Porter, FS Reintsema, CD Saab, T Schulz, N Serlemitsos, P Smith, R Ullom, JN Yoha, K AF Wikus, Patrick Rutherford, J. M. Adams, J. S. Bagdasarova, Y. Bandler, S. R. Bautz, M. Boyce, K. Brown, G. Deiker, S. Doriese, W. B. Figueroa-Feliciano, E. Flanagan, K. Galeazzi, M. Hilton, G. C. Hwang, U. Irwin, K. D. Kelley, R. L. Kallman, T. Kilbourne, C. A. Kissel, S. Leman, S. W. Levine, A. Loewenstein, M. Martinez-Galarce, D. Mushotzky, R. McCammon, D. Najjar, D. Petre, R. Porter, F. S. Reintsema, C. D. Saab, T. Schulz, N. Serlemitsos, P. Smith, R. Ullom, J. N. Yoha, K. TI Micro-X, the TES X-ray Imaging Rocket: First Year Progress SO IEEE TRANSACTIONS ON APPLIED SUPERCONDUCTIVITY LA English DT Article; Proceedings Paper CT Applied Superconductivity Conference CY AUG 17-22, 2008 CL Chicago, IL SP ATI Wah Chang, Coalit Commercial Applicat Superconductors, CryoZone, GE Global Res Ctr, IEEE Council Superconductiv, IEEE Magnet Soc, PHPK Technologies, SuperPower Inc, Teax Ctr Superconductiv, Univ Houston DE Cryogenics; rockets; SQUIDs; transition edge sensors; X-ray astronomy AB Micro-X is a sounding-rocket experiment that will combine a transition edge sensor (TES) microcalorimeter array with an imaging mirror to obtain high-spectral-resolution images of astronomical X-ray sources. The instrument's resolution across the 0.3-2.5 keV band will be 2 eV. The first flight will target the region of the Bright Eastern Knot of the Puppis A supernova remnant and is slated for January 2011. The obtained high-resolution X-ray spectra will be used to ascertain the temperature and ionization state of the X-ray-emitting gas and to determine its velocity structure. The TES array is read out by a time-division superconducting quantum interference device (SQUID) multiplexing system. The detector front end assembly and the SQUID multiplexing circuit are cooled to the operating temperature of 50 mK with an adiabatic demagnetization refrigerator (ADR). The design of this refrigerator is tailored to the requirements of rocket flight. Stable operation of the TES array close to the ADR magnet will be achieved with a magnetic shielding system, which will be based on a combination of a bucking coil and high-permeability and superconducting shield materials to cancel out residual fields. We describe our progress in developing the Micro-X instrument. C1 [Wikus, Patrick; Rutherford, J. M.; Bagdasarova, Y.; Bautz, M.; Figueroa-Feliciano, E.; Flanagan, K.; Kissel, S.; Leman, S. W.; Levine, A.; Najjar, D.; Schulz, N.] MIT, Cambridge, MA 02139 USA. [Adams, J. S.; Bandler, S. R.; Boyce, K.; Hwang, U.; Kelley, R. L.; Kallman, T.; Kilbourne, C. A.; Loewenstein, M.; Mushotzky, R.; Petre, R.; Porter, F. S.; Serlemitsos, P.; Smith, R.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Brown, G.] Lawrence Livermore Natl Lab, High Energy Dens Phys & Astrophys Div, Livermore, CA 94550 USA. [Deiker, S.; Martinez-Galarce, D.] Lockheed Martin Solar & Astrophys Lab, Palo Alto, CA 94304 USA. [Doriese, W. B.; Hilton, G. C.; Irwin, K. D.; Reintsema, C. D.; Ullom, J. N.] Natl Inst Stand & Technol, Boulder, CO 80305 USA. [Galeazzi, M.] Univ Miami, Dept Phys, Coral Gables, FL 33146 USA. [McCammon, D.] Univ Wisconsin, Dept Phys, Madison, WI 53706 USA. [Saab, T.; Yoha, K.] Univ Florida, Dept Phys, Gainesville, FL 32611 USA. RP Wikus, P (reprint author), MIT, 77 Massachusetts Ave, Cambridge, MA 02139 USA. EM wikus@mit.edu RI Bandler, Simon/A-6258-2010; Kelley, Richard/K-4474-2012; Porter, Frederick/D-3501-2012 OI Bandler, Simon/0000-0002-5112-8106; Porter, Frederick/0000-0002-6374-1119 NR 7 TC 1 Z9 1 U1 0 U2 4 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855 USA SN 1051-8223 J9 IEEE T APPL SUPERCON JI IEEE Trans. Appl. Supercond. PD JUN PY 2009 VL 19 IS 3 BP 553 EP 556 DI 10.1109/TASC.2009.2019129 PG 4 WC Engineering, Electrical & Electronic; Physics, Applied SC Engineering; Physics GA 474KK UT WOS:000268282000100 ER PT J AU Iyomoto, N Bandler, SR Brekosky, RP Brown, AD Chervenak, JA Eckart, ME 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. Eckart, M. E. Finkbeiner, F. M. Kelley, R. L. Kilbourne, C. A. Porter, F. S. Sadleir, J. E. Smith, S. J. TI Heat Sinking, Crosstalk, and Temperature Uniformity for Large Close-Packed Microcalorimeter Arrays SO IEEE TRANSACTIONS ON APPLIED SUPERCONDUCTIVITY LA English DT Article; Proceedings Paper CT Applied Superconductivity Conference CY AUG 17-22, 2008 CL Chicago, IL SP ATI Wah Chang, Coalit Commercial Applicat Superconductors, CryoZone, GE Global Res Ctr, IEEE Council Superconductiv, IEEE Magnet Soc, PHPK Technologies, SuperPower Inc, Teax Ctr Superconductiv, Univ Houston DE Microcalorimeters; transition-edge sensors; x-ray spectroscopy ID X-RAY MICROCALORIMETERS; ABSORBER DESIGN AB In a large close-packed array of x-ray microcalorimeters, sufficient heat sinking is important to minimize thermal crosstalk between pixels and to make the bath temperature of all the pixels uniform. We have measured crosstalk in our 8 x 8 pixel arrays. The shapes of the thermal crosstalk pulses are reproduced well as a convolution of heat input from the source pixel and the thermal decay in the receiver pixel. The amount of the thermal crosstalk is clearly dependent on the degree of electrothermal feedback. We have compared the magnitude of thermal crosstalk with and without a heat-sinking copper layer on the backside of the silicon frame as a function of distance between the source and receiver pixels. Using the results obtained, we have estimated the degradation of energy resolution that is expected as a function of count rate. We have also studied the temperature distribution within an array due to continuous heating from the TES bias to estimate impacts on the uniformity of the pixel performance. C1 [Iyomoto, N.] Univ Tokyo, Nucl Engn & Management Dept, Tokyo 1138656, Japan. [Iyomoto, N.; Bandler, S. R.; Brekosky, R. P.; Brown, A. -D.; Chervenak, J. A.; Eckart, M. E.; Finkbeiner, F. M.; Kelley, R. L.; Kilbourne, C. A.; Porter, F. S.; Sadleir, J. E.; Smith, S. J.] NASA, Greenbelt, MD 20771 USA. RP Iyomoto, N (reprint author), Univ Tokyo, Nucl Engn & Management Dept, Tokyo 1138656, Japan. EM iyomoto@n.t.u-tokyo.ac.jp; sbandler@milkyway.gsfc.nasa.gov; regis@lheapop.gsfc.nasa.gov; abrown@pop500.gsfc.nasa.gov; jcherven@pop500.gsfc.nasa.gov; eckart@milkyway.gsfc.nasa.gov; fmf@milkyway.gsfc.nasa.gov; kelley@lheapop.gsfc.nasa.gov; cak@milkyway.gsfc.nasa.gov; porter@milkyway.gsfc.nasa.gov; sadleir@milkyway.gsfc.nasa.gov; sjs@milkyway.gsfc.nasa.gov 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 6 TC 3 Z9 3 U1 0 U2 3 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 1051-8223 J9 IEEE T APPL SUPERCON JI IEEE Trans. Appl. Supercond. PD JUN PY 2009 VL 19 IS 3 BP 557 EP 560 DI 10.1109/TASC.2009.2017704 PN 1 PG 4 WC Engineering, Electrical & Electronic; Physics, Applied SC Engineering; Physics GA 474KK UT WOS:000268282000101 ER PT J AU Stevenson, TR Adams, JS Hsieh, WT Moseley, SH Travers, DE U-yen, K Wollack, EJ Zmuidzinas, J AF Stevenson, Thomas R. Adams, Joseph S. Hsieh, Wen-Ting Moseley, Samuel Harvey Travers, Douglas E. U-yen, Kongpop Wollack, Edward J. Zmuidzinas, Jonas TI Superconducting Films for Absorber-Coupled MKID Detectors for Sub-Millimeter and Far-Infrared Astronomy SO IEEE TRANSACTIONS ON APPLIED SUPERCONDUCTIVITY LA English DT Article; Proceedings Paper CT Applied Superconductivity Conference CY AUG 17-22, 2008 CL Chicago, IL SP ATI Wah Chang, Coalit Commercial Applicat Superconductors, CryoZone, GE Global Res Ctr, IEEE Council Superconductiv, IEEE Magnet Soc, PHPK Technologies, SuperPower Inc, Teax Ctr Superconductiv, Univ Houston DE Aluminum; inductance; microwave measurements; niobium; Q factor; superconducting resonators ID ALUMINUM AB We describe measurements of the properties, at dc, gigahertz, and terahertz frequencies, of thin (10 nm) aluminum films with 10 Omega/square normal state sheet resistance. Such films can be applied to construct microwave kinetic inductance detector arrays for submillimeter and far-infrared astronomical applications in which incident power excites quasiparticles directly in a superconducting resonator that is configured to present a matched-impedance to the high frequency radiation being detected. For films 10 nm thick, we report normal state sheet resistance, resistance-temperature curves for the superconducting transition, quality factor and kinetic inductance fraction for microwave resonators made from patterned films, and terahertz measurements of sheet impedance measured with a Fourier Transform Spectrometer. We compare properties with similar resonators made from niobium 600 nm thick. C1 [Stevenson, Thomas R.; Adams, Joseph S.; Hsieh, Wen-Ting; Moseley, Samuel Harvey; Travers, Douglas E.; U-yen, Kongpop; Wollack, Edward J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Zmuidzinas, Jonas] CALTECH, Dept Phys, Pasadena, CA 91125 USA. RP Stevenson, TR (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. EM Thomas.R.Stevenson@nasa.gov; Joseph.S.Adams@nasa.gov; wen-ting.hsieh-1@nasa.gov; harvey.moseley@nasa.gov; douglas.e.travers@nasa.gov; kongpop.u-yen-1@nasa.gov; edward.j.wol-lack@nasa.gov; jonas@caltech.edu RI Moseley, Harvey/D-5069-2012; Wollack, Edward/D-4467-2012 OI Wollack, Edward/0000-0002-7567-4451 NR 16 TC 4 Z9 4 U1 0 U2 4 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855 USA SN 1051-8223 J9 IEEE T APPL SUPERCON JI IEEE Trans. Appl. Supercond. PD JUN PY 2009 VL 19 IS 3 BP 561 EP 564 DI 10.1109/TASC.2009.2019661 PG 4 WC Engineering, Electrical & Electronic; Physics, Applied SC Engineering; Physics GA 474KK UT WOS:000268282000102 ER PT J AU Kumar, S Vayonakis, A LeDuc, HG Day, PK Golwala, S Zmuidzinas, J AF Kumar, Shwetank Vayonakis, Anastasios LeDuc, Henry G. Day, Peter K. Golwala, Sunil Zmuidzinas, Jonas TI Millimeter-Wave Lumped Element Superconducting Bandpass Filters for Multi-Color Imaging SO IEEE TRANSACTIONS ON APPLIED SUPERCONDUCTIVITY LA English DT Article; Proceedings Paper CT Applied Superconductivity Conference CY AUG 17-22, 2008 CL Chicago, IL SP ATI Wah Chang, Coalit Commercial Applicat Superconductors, CryoZone, GE Global Res Ctr, IEEE Council Superconductiv, IEEE Magnet Soc, PHPK Technologies, SuperPower Inc, Teax Ctr Superconductiv, Univ Houston DE Bandpass filters; passive microwave circuits; submillimeter astronomy AB The opacity due to water vapor in the Earth's atmosphere obscures portions of the sub-THz spectrum (mm/sub-mm wavelengths) to ground based astronomical observation. For maximum sensitivity, instruments operating at these wavelengths must be designed to have spectral responses that match the available windows in the atmospheric transmission that occur in between the strong water absorption lines. Traditionally, the spectral response of mm/sub-mm instruments has been set using optical, metal-mesh bandpass filters [1]. An alternative method for defining the passbands, available when using superconducting detectors coupled with planar antennas, is to use on-chip, superconducting filters [2]. This paper presents the design and testing of superconducting, lumped element, on-chip bandpass filters (BPFs), placed inline with the microstrip connecting the antenna and the detector, covering the frequency range from 209-416 GHz. Four filters were designed with pass bands 209-274 GHz, 265-315 GHz, 335-361 GHz and 397-416 GHz corresponding to the atmospheric transmission windows. Fourier transform spectroscopy was used to verify that the spectral response of the BPFs is well predicted by the computer simulations. Two-color operation of the pixels was demonstrated by connecting two detectors to a single broadband antenna through two BPFs. Scalability of the design to multiple (four) colors is discussed. C1 [Kumar, Shwetank] IBM Corp, Thomas J Watson Res Ctr, Yorktown Hts, NY 10598 USA. [Kumar, Shwetank] CALTECH, Dept Appl Phys, Pasadena, CA 91125 USA. [Vayonakis, Anastasios; Golwala, Sunil; Zmuidzinas, Jonas] CALTECH, Dept Phys, Pasadena, CA 91125 USA. [LeDuc, Henry G.; Day, Peter K.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Kumar, S (reprint author), IBM Corp, Thomas J Watson Res Ctr, Yorktown Hts, NY 10598 USA. EM shwetank@us.ibm.com; avayona@submm.caltech.edu; henry.g.leduc@jpl.nasa.gov; peter.k.day@jpl.nasa.gov; golwala@caltech.edu; jonas@caltech.edu NR 16 TC 10 Z9 10 U1 1 U2 5 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855 USA SN 1051-8223 J9 IEEE T APPL SUPERCON JI IEEE Trans. Appl. Supercond. PD JUN PY 2009 VL 19 IS 3 BP 924 EP 929 DI 10.1109/TASC.2009.2017884 PG 6 WC Engineering, Electrical & Electronic; Physics, Applied SC Engineering; Physics GA 474KK UT WOS:000268282000187 ER PT J AU Luongo, CA Masson, PJ Nam, T Mavris, D Kim, HD Brown, GV Waters, M Hall, D AF Luongo, Cesar A. Masson, Philippe J. Nam, Taewoo Mavris, Dimitri Kim, Hyun D. Brown, Gerald V. Waters, Mark Hall, David TI Next Generation More-Electric Aircraft: A Potential Application for HTS Superconductors SO IEEE TRANSACTIONS ON APPLIED SUPERCONDUCTIVITY LA English DT Article DE Aircraft; electric propulsion; superconducting motor ID CORED SYNCHRONOUS MACHINES; MOTOR; PROPULSION; DESIGN; WINDINGS; FLUX AB Sustainability in the aviation industry calls for aircraft that are significantly quieter and more fuel efficient than today's fleet. Achieving this will require revolutionary new concepts, in particular, electric propulsion. Superconducting machines offer the only viable path to achieve the power densities needed in airborne applications. This paper outlines the main issues involved in using superconductors for aeropropulsion. We review our investigation of the feasibility of superconducting electric propulsion, which integrate for the first time, the multiple disciplines and areas of expertise needed to design electric aircraft. It is shown that superconductivity is clearly the enabling technology for the more efficient turbo-electric aircraft of the future. C1 [Luongo, Cesar A.] Florida A&M Florida State Univ, Dept Mech Engn, Coll Engn, Tallahassee, FL 32307 USA. [Masson, Philippe J.] Ctr Adv Power Syst, Tallahassee, FL USA. [Masson, Philippe J.] Adv Magnet Lab, Palm Bay, FL USA. [Nam, Taewoo; Mavris, Dimitri] Georgia Inst Technol, Dept Aeronaut Engn, Aerosp Syst Design Lab, Atlanta, GA 30332 USA. [Kim, Hyun D.; Brown, Gerald V.] NASA, Glenn Res Ctr, Cleveland, OH USA. [Waters, Mark; Hall, David] DHC Engn, San Luis Obispo, CA USA. RP Luongo, CA (reprint author), Florida A&M Florida State Univ, Dept Mech Engn, Coll Engn, Tallahassee, FL 32307 USA. EM luongo@magnet.fsu.edu; pmasson@magnetlab.com; taewoo.nam@asdl.gatech.edu; Hyun.D.Kim@nasa.gov; Gerald.V.Brown@nasa.gov; mwaters@asdl.gatech.edu RI Masson, Philippe/G-6408-2012 FU NASA Fundamental Aeronautics Program; Department of Defense Research and Engineering (DDRE) FX Manuscript received September 05, 2008. First published June 30, 2009; current version published July 15, 2009. This work was supported by the NASA Fundamental Aeronautics Program and the Department of Defense Research and Engineering (DDR&E) division under the URETI on Aeropropulsion and Power. NR 36 TC 48 Z9 48 U1 4 U2 15 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855 USA SN 1051-8223 J9 IEEE T APPL SUPERCON JI IEEE Trans. Appl. Supercond. PD JUN PY 2009 VL 19 IS 3 BP 1055 EP 1068 DI 10.1109/TASC.2009.2019021 PG 14 WC Engineering, Electrical & Electronic; Physics, Applied SC Engineering; Physics GA 474KL UT WOS:000268282100001 ER PT J AU Makida, Y Yamamoto, A Yoshimura, K Tanaka, K Suzuki, J Matsuda, S Hasegawa, M Horikoshi, A Shinoda, R Sakai, K Mizumaki, S Orito, R Matsukawa, Y Kusumoto, A Mitchell, JW Streitmatter, RE Hams, T Sasaki, M Thakur, N AF Makida, Yasuhiro Yamamoto, Akira Yoshimura, Koji Tanaka, Ken-ichi Suzuki, Jun'ichi Matsuda, Shinya Hasegawa, Masata Horikoshi, Atsushi Shinoda, Ryoko Sakai, Kenichi Mizumaki, Shoichi Orito, Reiko Matsukawa, Yousuke Kusumoto, Akira Mitchell, John W. Streitmatter, Robert E. Hams, Thomas Sasaki, Makoto Thakur, Neeharika TI The BESS-Polar Ultra-Thin Superconducting Solenoid Magnet and Its Operational Characteristics During Long-Duration Scientific Ballooning Over Antarctica SO IEEE TRANSACTIONS ON APPLIED SUPERCONDUCTIVITY LA English DT Article DE Aluminum stabilized superconductor; balloon-borne experiment; BESS; detector magnet; thin solenoid ID PARTICLE ASTROPHYSICS AB An ultra-thin superconducting solenoid has been developed for a cosmic-ray spectrometer ballooning over Antarctica, which is named BESS-Polar II. The coil with a diameter of 0.9 m, a length of 1.4 m and a thickness of 3.5 mm, is wound with high-strength aluminum stabilized superconductor and provides 0.8 T in the spectrometer. Based on the experience at the BESS-Polar-I solenoid flight for nine days in 2004, the BESS-Polar-II solenoid, which was cryogenically improved, realized a persistent current mode operation for 25 days in the second flight campaign in December 2007 though January 2008. It has contributed to accumulate the cosmic-ray observation data with 4700 million events and 16 terabyte in a hard disk unit. This report will describe the second solenoid performance during the flight. C1 [Makida, Yasuhiro; Yamamoto, Akira; Yoshimura, Koji; Tanaka, Ken-ichi; Suzuki, Jun'ichi; Matsuda, Shinya; Hasegawa, Masata; Horikoshi, Atsushi] KEK, High Energy Accelerator Res Org, Tsukuba, Ibaraki 3050801, Japan. [Shinoda, Ryoko; Sakai, Kenichi] Univ Tokyo, Tokyo 1130033, Japan. [Mizumaki, Shoichi] Toshiba, Kanagawa 2300045, Japan. [Orito, Reiko; Matsukawa, Yousuke; Kusumoto, Akira] Kobe Univ, Kobe, Hyogo 6578501, Japan. [Mitchell, John W.; Streitmatter, Robert E.; Hams, Thomas; Sasaki, Makoto] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Thakur, Neeharika] Univ Denver, Denver, CO 80208 USA. RP Makida, Y (reprint author), KEK, High Energy Accelerator Res Org, Tsukuba, Ibaraki 3050801, Japan. EM yasuhiro.makida@kek.jp FU Japan MEXT FX work was supported by the Japan MEXT Grant-in-Aid and international collaboration with NASA/GDFC in the U. S. NR 9 TC 4 Z9 4 U1 1 U2 6 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855 USA SN 1051-8223 J9 IEEE T APPL SUPERCON JI IEEE Trans. Appl. Supercond. PD JUN PY 2009 VL 19 IS 3 BP 1315 EP 1319 DI 10.1109/TASC.2009.2017946 PG 5 WC Engineering, Electrical & Electronic; Physics, Applied SC Engineering; Physics GA 474KL UT WOS:000268282100055 ER PT J AU Zhang, H Mudawar, I Hasan, MM AF Zhang, Hui Mudawar, Issam Hasan, Mohammad M. TI Application of Flow Boiling for Thermal Management of Electronics in Microgravity and Reduced-Gravity Space Systems SO IEEE TRANSACTIONS ON COMPONENTS AND PACKAGING TECHNOLOGIES LA English DT Article DE Electronic cooling; microgravity; phase change ID CRITICAL HEAT-FLUX; TRIGGER MECHANISM; CHF MECHANISM; ORIENTATION; WALL; LENGTH; MODEL; LONG AB Large density differences between liquid and vapor create buoyancy effects in the presence of a gravitational field. Such effects can play an important role in two-phase fluid flow and heat transfer, especially critical heat flux (CHF). CHF poses significant risk to electronic devices, and the ability to predict its magnitude is crucial to both the safety and reliability of these devices. Variations in the gravitational field perpendicular to a flow boiling surface can take several forms, from flows at different orientations at to the microgravity environment of planetary orbit, to the reduced gravity on the Moon and Mars, and the high g's encountered in fighter aircraft during fast aerial maneuvers. While high coolant velocities can combat the detrimental effects of reduced gravity, limited power budget in space systems imposes stringent constraints on coolant flow rate. Thus, the task of dissipating the heat must be accomplished with the lowest possible flow velocity while safely avoiding CHF. In this paper, flow-boiling CHF is investigated on Earth as well as in reduced gravity parabolic flight experiments using FC-72 as working fluid. CHF showed sensitivity to gravity at low velocities, with microgravity yielding significantly lower CHF values compared to those at. Differences in CHF value decreased with increasing flow velocity until a velocity limit was reached above which the effects of gravity became inconsequential. This proves existing data, correlations, and models developed from studies can be employed with confidence to design reduced gravity thermal management systems, provided the flow velocity is maintained above this limit. This paper discusses two powerful predictive tools. The first, which consist of three dimensionless criteria, centers on determination of the velocity limit. The second is a theoretically based model for flow boiling CHF in reduced gravity below this velocity limit. C1 [Zhang, Hui; Mudawar, Issam] BTPFL, W Lafayette, IN 47907 USA. [Zhang, Hui; Mudawar, Issam] PUIECA, W Lafayette, IN 47907 USA. [Hasan, Mohammad M.] NASA, Glenn Res Ctr, Cleveland, OH 44134 USA. RP Zhang, H (reprint author), BTPFL, W Lafayette, IN 47907 USA. EM mu-dawar@ecn.purdue.edu FU National Aeronautics and Space Administration [NNC04GA54G] FX Manuscript received April 03, 2008; revised July 11, 2008. First published January 09, 2009; current version published July 22, 2009. This work was supported by the National Aeronautics and Space Administration under Grant NNC04GA54G. This work was recommended for publication by Associate Editor T. Lee upon evaluation of the reviewers comments. NR 20 TC 11 Z9 11 U1 0 U2 17 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855 USA SN 1521-3331 J9 IEEE T COMPON PACK T JI IEEE Trans. Compon. Packaging Technol. PD JUN PY 2009 VL 32 IS 2 BP 466 EP 477 DI 10.1109/TCAPT.2008.2004413 PG 12 WC Engineering, Manufacturing; Engineering, Electrical & Electronic; Materials Science, Multidisciplinary SC Engineering; Materials Science GA 474KS UT WOS:000268282800028 ER PT J AU Teverovsky, A AF Teverovsky, Alexander TI Scintillation Breakdowns and Reliability of Solid Tantalum Capacitors SO IEEE TRANSACTIONS ON DEVICE AND MATERIALS RELIABILITY LA English DT Article DE Capacitors; electric breakdown; reliability; reliability modeling ID DEPENDENT DIELECTRIC-BREAKDOWN; PENTOXIDE; MODEL AB Scintillations are momentarily local breakdowns in tantalum capacitors, which are often considered as nuisances rather than failures. However, this paper shows that scintillations are damaging for more than 30% of part types and up to 100% for some lots. Scintillations can be observed after many hours of operation, and the probability of repeat scintillations is higher than of the initial event. In this paper, a time-dependent scintillation breakdown is considered as one of the major reasons of failures during steady-state operation of the capacitors. Using a modified thermochemical model, the distribution of times to failure can be simulated based on the distribution of breakdown voltages. The analysis of distributions of scintillation breakdown voltages and the assessment of the safety margins are critical to assure high quality and reliability of tantalum capacitors. C1 NASA, Goddard Space Flight Ctr, Perot Syst, Greenbelt, MD 20771 USA. RP Teverovsky, A (reprint author), NASA, Goddard Space Flight Ctr, Perot Syst, Greenbelt, MD 20771 USA. EM Alexander.A.Teverovsky@nasa.gov FU NASA Electronic Parts and Packaging (NEPP) Program FX Manuscript received February 10, 2009. First published April 7, 2009: current version published June 5, 2009. This work was supported by NASA Electronic Parts and Packaging (NEPP) Program. NR 18 TC 3 Z9 3 U1 0 U2 3 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855 USA SN 1530-4388 J9 IEEE T DEVICE MAT RE JI IEEE Trans. Device Mater. Reliab. PD JUN PY 2009 VL 9 IS 2 BP 318 EP 324 DI 10.1109/TDMR.2009.2020153 PG 7 WC Engineering, Electrical & Electronic; Physics, Applied SC Engineering; Physics GA 454ZC UT WOS:000266722900029 ER PT J AU Enjolras, VM Rodriguez, E AF Enjolras, Vivien M. Rodriguez, Ernesto TI An Assessment of a Ka-Band Radar Interferometer Mission Accuracy Over Eurasian Rivers SO IEEE TRANSACTIONS ON GEOSCIENCE AND REMOTE SENSING LA English DT Article DE Europe; hydrology; interferometry ID TOPEX/POSEIDON SATELLITE ALTIMETRY; LEVEL FLUCTUATIONS; WATER-RESOURCES; SAR IMAGERY; SURFACE; OCEAN; STATISTICS; SYSTEM; BASIN AB The Water Elevation Recovery satellite mission is dedicated to the determination of land surface water extent, elevation, and slope using a Ka-band radar interferometer (KaRIn) as its primary instrument. Determining these parameters to the accuracy desired for hydrologic applications is challenging. The scientific objectives of the mission have been set up to 10 cm for the height budget and 10 mu rad (1 cm/1 km) for the slope budget. In this paper, we implement a Virtual Mission simulation and use it to examine the measurement performances for three case studies in Europe: a relatively small river such as the Meuse in Northern Western Europe, the Lena river in Russia, one of the major Siberian rivers, and Lake Leman in Western Europe. We simulate KaRIn data with the associated instrument and geophysical error sources and implement ground processing techniques to go from the original raw data to science data. We examine the impact of external errors in detail and implement calibration techniques that rely on the use of ancillary topographic data, such as the Shuttle Radar Topography Mission digital elevation model (DEM). We find that the impact of external errors can be reduced to a few centimeters. The random error budget can also be reduced below 10 cm by means of appropriate processing. The scientific requirements of the mission are shown to be met for all cases. C1 [Enjolras, Vivien M.] Thales Alenia Space, Business Unit Observat Syst & Radars, F-31037 Toulouse, France. [Rodriguez, Ernesto] NASA, Jet Prop Lab, Pasadena, CA 91109 USA. RP Enjolras, VM (reprint author), Thales Alenia Space, Business Unit Observat Syst & Radars, F-31037 Toulouse, France. EM vivien.enjolras@thalesaleniaspace.com; ernesto.rodriguez@jpl.nasa.gov FU CNES; Thales Alenia Space; NASA Jet Propulsion Laboratory FX This work was supported in part by CNES, by Thales Alenia Space, and by the NASA Jet Propulsion Laboratory. NR 44 TC 6 Z9 6 U1 0 U2 3 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 JUN PY 2009 VL 47 IS 6 BP 1752 EP 1765 DI 10.1109/TGRS.2008.2006370 PG 14 WC Geochemistry & Geophysics; Engineering, Electrical & Electronic; Remote Sensing; Imaging Science & Photographic Technology SC Geochemistry & Geophysics; Engineering; Remote Sensing; Imaging Science & Photographic Technology GA 450NW UT WOS:000266409100017 ER PT J AU West, RD Anderson, Y Boehmer, R Borgarelli, L Callahan, P Elachi, C Gim, Y Hamilton, G Hensley, S Janssen, MA Johnson, WTK Kelleher, K Lorenz, R Ostro, S Roth, L Shaffer, S Stiles, B Wall, S Wye, LC Zebker, HA AF West, Richard D. Anderson, Yanhua Boehmer, Rudy Borgarelli, Leonardo Callahan, Philip Elachi, Charles Gim, Yonggyu Hamilton, Gary Hensley, Scott Janssen, Michael A. Johnson, William T. K. Kelleher, Kathleen Lorenz, Ralph Ostro, Steve Roth, Ladislav Shaffer, Scott Stiles, Bryan Wall, Steve Wye, Lauren C. Zebker, Howard A. TI Cassini RADAR Sequence Planning and Instrument Performance SO IEEE TRANSACTIONS ON GEOSCIENCE AND REMOTE SENSING LA English DT Article DE Cassini; RADAR; radiometer; synthetic aperture radar (SAR) ID TITANS SURFACE; SCATTEROMETER; REFLECTIVITY AB The Cassini RADAR is a multimode instrument used to map the surface of Titan, the atmosphere of Saturn, the Saturn ring system, and to explore the properties of the icy satellites. Four different active mode bandwidths and a passive radiometer mode provide a wide range of flexibility in taking measurements. The scatterometer mode is used for real aperture imaging of Titan, high-altitude (around 20000 km) synthetic aperture imaging of Titan and Iapetus, and long range (up to 700000 km) detection of disk integrated albedos for satellites in the Saturn system. Two SAR modes are used for high- and medium-resolution (300-1000 m) imaging of Titan's surface during close flybys. A high-bandwidth altimeter mode is used for topographic profiling in selected areas with a range resolution of about 35 m. The passive radiometer mode is used to map emission from Titan, from Saturn's atmosphere, from the rings, and from the icy satellites. Repeated scans with differing polarizations using both active and passive data provide data that can usefully constrain models of surface composition and structure. The radar and radiometer receivers show very good stability, and calibration observations have provided an absolute calibration good to about 1.3 dB. Relative uncertainties within a pass and between passes can be even smaller. Data are currently being processed and delivered to the planetary data system at quarterly intervals one year after being acquired. C1 [West, Richard D.; Anderson, Yanhua; Boehmer, Rudy; Callahan, Philip; Elachi, Charles; Gim, Yonggyu; Hamilton, Gary; Hensley, Scott; Janssen, Michael A.; Johnson, William T. K.; Kelleher, Kathleen; Ostro, Steve; Roth, Ladislav; Shaffer, Scott; Stiles, Bryan; Wall, Steve] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Borgarelli, Leonardo] Thales Alenia Space Italia, I-00131 Rome, Italy. [Lorenz, Ralph] Johns Hopkins Univ, Appl Phys Lab, Baltimore, MD 21218 USA. [Wye, Lauren C.; Zebker, Howard A.] Stanford Univ, Stanford, CA 94305 USA. RP West, RD (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM richard.west@jpl.nasa.gov; yanhua.anderson@jpl.nasa.gov; rboehmer@jpl.nasa.gov; l.borgarelli@roma.alespazio.it; phil.callahan@jpl.nasa.gov; charles.elachi@jpl.nasa.gov; yonggyu.gim@jpl.nasa.gov; gary.hamilton@jpl.nasa.gov; scott.hensley@jpl.nasa.gov; mike.janssen@jpl.nasa.gov; wtk.johnson@jpl.nasa.gov; kathleen.kelleher@jpl.nasa.gov; ralph.lorenz@jhuapl.edu; ladislav.roth@jpl.nasa.gov; scott.shaffer@jpl.nasa.gov; bryan.stiles@jpl.nasa.gov; steve.wall@jpl.nasa.gov; lcwye@stanford.edu; zebker@stanford.edu RI Lorenz, Ralph/B-8759-2016 OI Lorenz, Ralph/0000-0001-8528-4644 FU NASA FX This work was performed at the JPL, California Institute of Technology, under contract with the NASA. NR 23 TC 13 Z9 13 U1 0 U2 4 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 0196-2892 J9 IEEE T GEOSCI REMOTE JI IEEE Trans. Geosci. Remote Sensing PD JUN PY 2009 VL 47 IS 6 BP 1777 EP 1795 DI 10.1109/TGRS.2008.2007217 PG 19 WC Geochemistry & Geophysics; Engineering, Electrical & Electronic; Remote Sensing; Imaging Science & Photographic Technology SC Geochemistry & Geophysics; Engineering; Remote Sensing; Imaging Science & Photographic Technology GA 450NW UT WOS:000266409100019 ER PT J AU Enjolras, VM Rodriguez, E AF Enjolras, Vivien M. Rodriguez, Ernesto TI Using Altimetry Waveform Data and Ancillary Information From SRTM, Landsat, and MODIS to Retrieve River Characteristics SO IEEE TRANSACTIONS ON GEOSCIENCE AND REMOTE SENSING LA English DT Article DE Altimetry; Europe; hydrology; waveform ID TOPEX/POSEIDON SATELLITE ALTIMETRY; LEVEL FLUCTUATIONS; AMAZON BASIN; SURFACE; OCEAN AB In this paper, spaceborne radar altimeters are shown to have the potential for monitoring the height of large rivers with accuracies of approximately 1 m. However, the need for a better height accuracy and the observations of smaller continental basins have led to studies on how to improve and extend the use of nadir-altimeter data. Conventional retracking techniques over land are limited to the examination of altimeter waveforms on a case-by-case basis. Due to the arbitrary geometry which may be present at altimeter river crossings, this approach may be limited to large rivers, which approximate ocean crossings. To overcome this limitation, we introduce a waveform-fitting method which uses the entire set of waveforms associated with a water crossing, rather than individual waveforms. By using ancillary data, such as digital elevation model (obtained from Shuttle Radar Topography Mission and Gtopo30) and classification maps (obtained from Landsat and MODIS), it is possible to recast the retracking problems as a maximum-likelihood-estimation problem. Theoretical power returns based on the a priori knowledge of the observed scenes are generated, resulting in a parametric library of waveform histories, which is then used to constrain the estimation. For demonstration, we concentrate on the river Meuse in northern western Europe and on the river Lena in Russia. The Meuse has important social impact, since it has flooded in the past and better real-time predictions of its changing stage may improve flood-forecasting skill. Furthermore, it presents a challenge to conventional nadir-altimeter waveform retracking. We will present both theoretical performance results and demonstrate the feasibility based on real altimeter data. C1 [Enjolras, Vivien M.] Thales Alenia Space, Business Unit Observat Syst & Radar, F-31037 Toulouse 1, France. [Rodriguez, Ernesto] CALTECH, Jet Prop Lab, Radar Sci & Engn Sect, Pasadena, CA 91125 USA. RP Enjolras, VM (reprint author), Thales Alenia Space, Business Unit Observat Syst & Radar, F-31037 Toulouse 1, France. EM vivien.enjolras@thalesaleniaspace.com FU CNES; Thales Alenia Space FX Manuscript received November 16. 2007; revised February 29, 2008 and June 25, 2008. First published February 3, 2009: Current version published May 22, 2009. The work of V. M. Enjolras was supported by in part by CNES and in part by Thales Alenia Space. NR 22 TC 6 Z9 6 U1 0 U2 5 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 JUN PY 2009 VL 47 IS 6 BP 1869 EP 1881 DI 10.1109/TGRS.2008.2006365 PG 13 WC Geochemistry & Geophysics; Engineering, Electrical & Electronic; Remote Sensing; Imaging Science & Photographic Technology SC Geochemistry & Geophysics; Engineering; Remote Sensing; Imaging Science & Photographic Technology GA 450NW UT WOS:000266409100026 ER PT J AU Cooper, M Fridman, G Staack, D Gutsol, AF Vasilets, VN Anandan, S Cho, YI Fridman, A Tsapin, A AF Cooper, Moogega Fridman, Gregory Staack, David Gutsol, Alexander F. Vasilets, Victor N. Anandan, Shivanthi Cho, Young I. Fridman, Alexander Tsapin, Alexandre TI Decontamination of Surfaces From Extremophile Organisms Using Nonthermal Atmospheric-Pressure Plasmas SO IEEE TRANSACTIONS ON PLASMA SCIENCE LA English DT Article DE Atmospheric-pressure discharges; cold plasma; dielectric barrier discharges (DBDs); plasma decontamination; sterilization ID DEINOCOCCUS-RADIODURANS; STERILIZATION; RADIATION; SURVIVAL AB We showed that nonthermal dielectric barrier discharge (DBD) plasma compromises the integrity of the cell membrane of Deinococcus radiodurans, an extremophile organism. In samples of D. radiodurans, which were dried in a laminar flow hood, we observe that DBD plasma exposure resulted in a six-log reduction in CFU (colony-forming unit) count after 30 min of treatment. When the Deinococcus radiodurans cells were suspended in distilled water and treated, it took only 15 s to achieve a four-log reduction of CFU count. C1 [Cooper, Moogega; Fridman, Alexander] Drexel Univ, Dept Mech Engn & Mech, AJ Drexel Plasma Inst, Philadelphia, PA 19104 USA. [Fridman, Gregory] Drexel Univ, Sch Biomed Engn Sci & Hlth Syst, Philadelphia, PA 19104 USA. [Staack, David] Texas A&M Univ, Dept Mech Engn, College Stn, TX 77843 USA. [Gutsol, Alexander F.] Chevron Corp, Chevron Energy Technol Co, Richmond, CA 94801 USA. [Vasilets, Victor N.] Russian Acad Sci, Inst Energy Problems Chem Phys, Chernogolovka 142432, Russia. [Anandan, Shivanthi] Drexel Univ, Dept Biosci & Biotechnol, Philadelphia, PA 19104 USA. [Tsapin, Alexandre] CALTECH, Jet Prop Lab, NASA, Pasadena, CA 91109 USA. RP Cooper, M (reprint author), Drexel Univ, Dept Mech Engn & Mech, AJ Drexel Plasma Inst, Philadelphia, PA 19104 USA. EM moogega@drexel.edu; greg.fridman@drexel.edu; dstaack@tamu.edu; AlexanderGutsol@chevron.com; vnvasilets@gmail.com; anandans@drexel.edu; choyi@drexel.edu; af55@drexel.edu; tsapin@jpl.nasa.gov RI Staack, David/A-5430-2010; Vasilets, Victor/I-2643-2014; OI Vasilets, Victor/0000-0002-7185-6768 FU National Aeronautics and Space Administration (NASA) [NNH04ZSS001N] FX This work was supported in part by the National Aeronautics and Space Administration (NASA) under Grant NNH04ZSS001N. A. Tsapin's contribution to the research described in this paper was carried out at the Jet Propulsion Laboratory, California Institute of Technology, Pasadena, under a contract with the NASA. NR 14 TC 26 Z9 27 U1 1 U2 14 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855 USA SN 0093-3813 J9 IEEE T PLASMA SCI JI IEEE Trans. Plasma Sci. PD JUN PY 2009 VL 37 IS 6 BP 866 EP 871 DI 10.1109/TPS.2008.2010618 PG 6 WC Physics, Fluids & Plasmas SC Physics GA 456UW UT WOS:000266877900021 ER PT J AU Patil, N Celaya, J Das, D Goebel, K Pecht, M AF Patil, Nishad Celaya, Jose Das, Diganta Goebel, Kai Pecht, Michael TI Precursor Parameter Identification for Insulated Gate Bipolar Transistor (IGBT) Prognostics SO IEEE TRANSACTIONS ON RELIABILITY LA English DT Article CT International Conference on Prognostics and Health Management CY OCT 06-09, 2008 CL Denver, CO SP IEEE DE Insulated gate bipolar transistors; precursors; prognostics AB Precursor parameters have been identified to enable development of a prognostic approach for insulated gate bipolar transistors (IGBT). The IGBT were subjected to thermal over-stress tests using a transistor test board until device latch-up. The collector-emitter current, transistor case temperature, transient and steady state gate voltages, and transient and steady state collector-emitter voltages were monitored in-situ during the test. Pre- and post-aging characterization tests were performed on the IGBT. The aged parts were observed to have shifts in capacitance-voltage (C-V) measurements as a result or trapped charge in the gate oxide. The collector-emitter ON voltage V(CE(ON)) showed a reduction with aging. The reduction in the V(CE(ON)) was found to be correlated to die attach degradation, as observed by scanning acoustic microscopy (SAM) analysis. The collector-emitter voltage, and transistor turn-off time were observed to be precursor parameters to latch-up. The monitoring of these precursor parameters will enable the development of a prognostic methodology for IGBT failure. The prognostic methodology will involve trending precursor data, and using physics of failure models for prediction of the remaining useful life of these devices. C1 [Patil, Nishad; Das, Diganta; Pecht, Michael] Univ Maryland, CALCE, College Pk, MD 20742 USA. [Celaya, Jose] NASA, Ames Res Ctr, SGT Inc, Moffett Field, CA 94035 USA. RP Patil, N (reprint author), Univ Maryland, CALCE, College Pk, MD 20742 USA. EM nishad@calce.umd.edu; Jose.R.Celaya@nasa.gov; digudas@calce.umd.edu; kai.goebel@nasa.gov; pech@calce.umd.edu OI Pecht, Michael/0000-0003-1126-8662 NR 13 TC 54 Z9 62 U1 1 U2 18 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855 USA SN 0018-9529 J9 IEEE T RELIAB JI IEEE Trans. Reliab. PD JUN PY 2009 VL 58 IS 2 BP 271 EP 276 DI 10.1109/TR.2009.2020134 PG 6 WC Computer Science, Hardware & Architecture; Computer Science, Software Engineering; Engineering, Electrical & Electronic SC Computer Science; Engineering GA 456UR UT WOS:000266877400004 ER PT J AU Turyshev, SG Shao, M Girerd, A Lane, B AF Turyshev, Slava G. Shao, Michael Girerd, Andre Lane, Benjamin TI A SEARCH FOR NEW PHYSICS WITH THE BEACON MISSION SO INTERNATIONAL JOURNAL OF MODERN PHYSICS D LA English DT Article DE Fundamental physics; tests of general relativity, scalar-tensor theories; modified gravity; interplanetary laser ranging; optical interferometry; BEACON mission ID VERIFICATION; GRAVITY AB The primary objective of the Beyond Einstein Advanced Coherent Optical Network ( BEACON) mission is a search for new physics beyond general relativity by measuring the curvature of relativistic space-time around the Earth. This curvature is characterized by the Eddington parameter gamma - the most fundamental relativistic gravity parameter and a direct measure for the presence of new physical interactions. BEACON will achieve an accuracy of 1 x 10(-9) in measuring the parameter., thereby going a factor of 30,000 beyond the present best result involving the Cassini spacecraft. Secondary mission objectives include: (i) a direct measurement of the "frame-dragging" and geodetic precessions in the Earth's rotational gravitomagnetic field, to 0.05% and 0.03% accuracy respectively, (ii) the first measurement of gravity's nonlinear effects on light and the corresponding second order spatial metric's effects to 0.01% accuracy. BEACON will lead to robust advances in tests of fundamental physics - this mission could discover a violation or extension of general relativity and/or reveal the presence of an additional long range interaction in physics. It will provide crucial information to separate modern scalar-tensor theories of gravity from general relativity, probe possible ways for gravity quantization, and test modern theories of cosmological evolution. C1 [Turyshev, Slava G.; Shao, Michael; Girerd, Andre] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Lane, Benjamin] Charles Stark Draper Lab Inc, Cambridge, MA 02139 USA. RP Turyshev, SG (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM turyshev@jpl.nasa.gov NR 14 TC 13 Z9 14 U1 0 U2 1 PU WORLD SCIENTIFIC PUBL CO PTE LTD PI SINGAPORE PA 5 TOH TUCK LINK, SINGAPORE 596224, SINGAPORE SN 0218-2718 J9 INT J MOD PHYS D JI Int. J. Mod. Phys. D PD JUN PY 2009 VL 18 IS 6 BP 1025 EP 1038 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 469BC UT WOS:000267868900008 ER PT J AU Fuster, D Bague, A Boeck, T Le Moyne, L Leboissetier, A Popinet, S Ray, P Scardovelli, R Zaleski, S AF Fuster, Daniel Bague, Anne Boeck, Thomas Le Moyne, Luis Leboissetier, Anthony Popinet, Stephane Ray, Pascal Scardovelli, Ruben Zaleski, Stephane TI Simulation of primary atomization with an octree adaptive mesh refinement and VOF method SO INTERNATIONAL JOURNAL OF MULTIPHASE FLOW LA English DT Article DE Atomization; Numerical simulation; Gerris; VOF; Two-phase mixing layer; Kelvin-Helmholtz ID NAVIER-STOKES EQUATIONS; 2-PHASE MIXING LAYERS; LEVEL SET METHOD; OF-FLUID METHOD; SURFACE-TENSION; MOVING INTERFACES; VOLUME FRACTIONS; LIQUID SHEET; FLOWS; GRIDS AB We present different simulations of primary atomization using an adaptive Volume-of-Fluid method based on octree meshes. The use of accurate numerical schemes for mesh adaptation, Volume-of-Fluid advection and balanced force surface tension calculation implemented in Gerris, the code used to perform the simulations included in this work. has made possible to carry out accurate simulations with characteristic scales spreading over several orders of magnitude. The code is validated by comparisons with the temporal linear theory for moderate density and viscosity ratios, which basically corresponds to atomization processes in high pressure chambers. In order to show the potential of the code in different scenarios related to atomization, preliminary results are shown in relation with the study of the two-dimensional and 3D temporal and spatial problem, the influence of the injector and the vortex generated inside the chamber, and the effect of swirling at high Reynolds numbers. (C) 2009 Elsevier Ltd. All rights reserved. C1 [Fuster, Daniel; Bague, Anne; Le Moyne, Luis; Ray, Pascal; Zaleski, Stephane] Univ Paris 06, UPMC, UMR 7190, Inst Jean Le Rond Alembert, F-75005 Paris, France. [Fuster, Daniel; Bague, Anne; Le Moyne, Luis; Ray, Pascal; Zaleski, Stephane] CNRS, UMR 7190, Inst Jean Le Rond Alembert, F-75005 Paris, France. [Boeck, Thomas] TU Ilmenau, Fachgebiet Thermo & Fluiddynam, D-98684 Ilmenau, Germany. [Leboissetier, Anthony] NASA, GISS, New York, NY 10025 USA. [Popinet, Stephane] NIWA, Wellington, New Zealand. [Scardovelli, Ruben] Univ Bologna, DIENCA, Lab Montecuccolino, Bologna, Italy. RP Fuster, D (reprint author), Univ Paris 06, UPMC, UMR 7190, Inst Jean Le Rond Alembert, F-75005 Paris, France. EM fuster@lmm.jussieu.fr RI Fuster, Daniel/K-8779-2014; Scardovelli, Ruben/P-9270-2015; Boeck, Thomas/C-2188-2017 OI Scardovelli, Ruben/0000-0002-1009-2434; Boeck, Thomas/0000-0002-0814-7432 NR 66 TC 80 Z9 81 U1 1 U2 45 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0301-9322 J9 INT J MULTIPHAS FLOW JI Int. J. Multiph. Flow PD JUN PY 2009 VL 35 IS 6 BP 550 EP 565 DI 10.1016/j.ijmultiphaseflow.2009.02.014 PG 16 WC Mechanics SC Mechanics GA 453WH UT WOS:000266643100007 ER PT J AU Conway, EM AF Conway, Erik M. TI Digital Apollo: Human and Machine in Spaceflight SO ISIS LA English DT Book Review C1 [Conway, Erik M.] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. RP Conway, EM (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0021-1753 EI 1545-6994 J9 ISIS JI Isis PD JUN PY 2009 VL 100 IS 2 BP 441 EP 442 PG 2 WC History & Philosophy Of Science SC History & Philosophy of Science GA 457DF UT WOS:000266905400076 ER PT J AU Wolff, DB Fisher, BL AF Wolff, David B. Fisher, Brad L. TI Assessing the Relative Performance of Microwave-Based Satellite Rain-Rate Retrievals Using TRMM Ground Validation Data SO JOURNAL OF APPLIED METEOROLOGY AND CLIMATOLOGY LA English DT Article ID MEASURING MISSION TRMM; TROPICAL RAINFALL; PASSIVE MICROWAVE; PRECIPITATION RADAR; UNITED-STATES; AMSR-E; SSM/I; ALGORITHMS; INFORMATION; SENSORS AB Spaceborne microwave sensors provide critical rain information used in several global multisatellite rain products, which in turn are used for a variety of important studies, including landslide forecasting, flash flood warning, data assimilation, climate studies, and validation of model forecasts of precipitation. This study employs 4 yr (2003-06) of satellite data to assess the relative performance and skill of the Special Sensor Microwave Imager [SSM/I (F13, F14, and F15], Advanced Microwave Sounding Unit [AMSU-B (N15, N16, and N17)], Advanced Microwave Scanning Radiometer for Earth Observing System [AMSR-E (Aqua)], and the Tropical Rainfall Measuring Mission (TRMM) Microwave Imager (TMI) in estimating surface rainfall based on direct instantaneous comparisons with ground-based rain estimates from the TRMM Ground Validation (GV) sites at Kwajalein, Republic of the Marshall Islands (KWAJ), and Melbourne, Florida (MELB). The relative performance of each of these satellite estimates is examined via comparisons with space-and time-coincident GV radar-based rain-rate estimates. Because underlying surface terrain is known to affect the relative performance of the satellite algorithms, the data for MELB were further stratified into ocean, land, and coast categories using a 0.25 degrees terrain mask. Of all the satellite estimates compared in this study, TMI and AMSR-E exhibited considerably higher correlations and skills in estimating-observing surface precipitation. While SSM/I and AMSU-B exhibited lower correlations and skills for each of the different terrain categories, the SSM/I absolute biases trended slightly lower than AMSR-E over ocean, where the observations from both emission and scattering channels were used in the retrievals. AMSU-B exhibited the least skill relative to GV in all of the relevant statistical categories, and an anomalous spike was observed in the probability distribution functions near 1.0 mm h(-1). This statistical artifact appears to be related to attempts by algorithm developers to include some lighter rain rates, not easily detectable by its scatter-only frequencies. AMSU-B, however, agreed well with GV when the matching data were analyzed on monthly scales. These results signal to developers of global rainfall products, such as the TRMM Multisatellite Precipitation Analysis (TMPA) and the Climate Data Center's Morphing (CMORPH) technique, that care must be taken when incorporating data from these input satellite estimates to provide the highest-quality estimates in their products. C1 [Wolff, David B.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Sci Syst & Applicat Inc, Lanham, MD USA. RP Wolff, DB (reprint author), NASA, Goddard Space Flight Ctr, Code 613-1, Greenbelt, MD 20771 USA. EM david.b.wolff@nasa.gov RI Wolff, David/H-5502-2012 FU National Aeronautics and Space Administration (NASA) [NNG07EJ50C] FX National Aeronautics and Space Administration (NASA) Grant NNG07EJ50C funded this study. The authors thank Dr. Ramesh Kakar (NASA Headquarters), Dr. ScottBraun (TRMM Project Scientist), Dr. Arthur Hou (GPM Project Scientist), and Mr. Richard Lawrence (Chief, TRMM Satellite Validation Office) for their support of this effort. We also greatly appreciate the efforts of Dr. Erich Stocker of the TRMM Science and Data Information System (TSDIS) and NASA Precipitation Processing System (PPS) for generating the quarter-degree TRMM data used in this study. We also thank the support staff of the TRMM Ground Validation program at NASA GSFC, especially David Marks, David Silberstein, Jason Pippitt, and David Makofski. NR 34 TC 29 Z9 29 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 JUN PY 2009 VL 48 IS 6 BP 1069 EP 1099 DI 10.1175/2008JAMC2127.1 PG 31 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 472JF UT WOS:000268125900001 ER PT J AU Polk, JE Mikellides, IG Katz, I Capece, AM AF Polk, James E. Mikellides, Ioannis G. Katz, Ira Capece, Angela M. TI Tungsten and barium transport in the internal plasma of hollow cathodes SO JOURNAL OF APPLIED PHYSICS LA English DT Article ID IMPREGNATED-CATHODE; OPERATION; MECHANISM; LIFE; BA AB The effect of tungsten erosion, transport, and redeposition on the operation of dispenser hollow cathodes was investigated in detailed examinations of the discharge cathode inserts from 8200 h and 30 352 h ion engine wear tests. Erosion and subsequent redeposition of tungsten in the electron emission zone at the downstream end of the insert reduce the porosity of the tungsten matrix, preventing the flow of barium from the interior. This inhibits the interfacial reactions of the barium-calcium-aluminate impregnant with the tungsten in the pores. A numerical model of barium transport in the internal xenon discharge plasma shows that the barium required to reduce the work function in the emission zone can be supplied from upstream through the gas phase. Barium that flows out of the pores of the tungsten insert is rapidly ionized in the xenon discharge and pushed back to the emitter surface by the electric field and drag from the xenon ion flow. This barium ion flux is sufficient to maintain a barium surface coverage at the downstream end greater than 0.6, even if local barium production at that point is inhibited by tungsten deposits. The model also shows that the neutral barium pressure exceeds the equilibrium vapor pressure of the impregnant decomposition reaction over much of the insert length, so the reactions are suppressed. Only a small region upstream of the zone blocked by tungsten deposits is active and supplies the required barium. These results indicate that hollow cathode failure models based on barium depletion rates in vacuum dispenser cathodes are very conservative. (c) 2009 American Institute of Physics. [DOI: 10.1063/1.3111970] C1 [Polk, James E.; Mikellides, Ioannis G.; Katz, Ira] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Capece, Angela M.] CALTECH, Pasadena, CA 91125 USA. RP Polk, JE (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM james.e.polk@jpl.nasa.gov FU National Aeronautics and Space Administration FX The authors would like to thank Al Owens, Ray Swindlehurst, and Ron Watkins for their assistance in preparing the test facility and Ron Ruiz and Jim Kulleck for their contributions in electron microscopy. The research described in this paper was carried out by the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. NR 24 TC 6 Z9 6 U1 1 U2 11 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 JUN 1 PY 2009 VL 105 IS 11 AR 113301 DI 10.1063/1.3111970 PG 13 WC Physics, Applied SC Physics GA 458VG UT WOS:000267053200025 ER PT J AU Young, SA Vaughan, MA AF Young, Stuart A. Vaughan, Mark A. TI The Retrieval of Profiles of Particulate Extinction from Cloud-Aerosol Lidar Infrared Pathfinder Satellite Observations (CALIPSO) Data: Algorithm Description SO JOURNAL OF ATMOSPHERIC AND OCEANIC TECHNOLOGY LA English DT Article ID TROPOSPHERIC AEROSOLS; BACKSCATTER; INVERSION AB This work describes the algorithms used for the fully automated retrieval of profiles of particulate extinction coefficients from the attenuated backscatter data acquired by the lidar on board the Cloud-Aerosol Lidar Infrared Pathfinder Satellite Observations (CALIPSO) spacecraft. The close interaction of the Hybrid Extinction Retrieval Algorithms (HERA) with the preceding processes that detect and classify atmospheric features (i.e., cloud and aerosol layers) is described within the context of the analysis of measurements from scenes of varying complexity. Two main components compose HERA: a top-level algorithm that selects the analysis pathway, the order of processing, and the analysis parameters, depending on the nature and spatial extent of the atmospheric features to be processed; and a profile solver or "extinction engine,'' whose task it is to retrieve profiles of particulate extinction and backscatter coefficients from specified sections of an atmospheric scene defined by the top-level algorithm. The operation of these components is described using synthetic data derived from Lidar In Space Technology Experiment (LITE) measurements. The performance of the algorithms is illustrated using CALIPSO measurements acquired during the mission on 1 January 2007. C1 [Young, Stuart A.] CSIRO Marine & Atmospher Res, Aspendale, Vic 3195, Australia. [Vaughan, Mark A.] NASA, Hampton, VA USA. RP Young, SA (reprint author), CSIRO Marine & Atmospher Res, Aspendale, Vic 3195, Australia. EM stuart.young@csiro.au RI Young, Stuart/A-8641-2011 OI Young, Stuart/0000-0001-6434-9816 FU NASA Langley Atmospheric Sciences Data Center FX The authors are pleased to acknowledge helpful comments on the manuscript from the authors of the companion algorithms in the extinction retrieval process. The CALIPSO data used in this paper were obtained from the NASA Langley Atmospheric Sciences Data Center. NR 39 TC 159 Z9 160 U1 9 U2 32 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 JUN PY 2009 VL 26 IS 6 BP 1105 EP 1119 DI 10.1175/2008JTECHA1221.1 PG 15 WC Engineering, Ocean; Meteorology & Atmospheric Sciences SC Engineering; Meteorology & Atmospheric Sciences GA 462RB UT WOS:000267372200006 ER PT J AU Tokay, A Hartmann, P Battaglia, A Gage, KS Clark, WL Williams, CR AF Tokay, Ali Hartmann, Peter Battaglia, Alessandro Gage, Kenneth S. Clark, Wallace L. Williams, Christopher R. TI A Field Study of Reflectivity and Z-R Relations Using Vertically Pointing Radars and Disdrometers SO JOURNAL OF ATMOSPHERIC AND OCEANIC TECHNOLOGY LA English DT Article ID RAIN-GAUGE MEASUREMENTS; DROP SIZE DISTRIBUTION; INSTRUMENTAL UNCERTAINTIES; CONVECTIVE CLOUDS; SPECTRA; DISTRIBUTIONS; CALIBRATION; ERRORS AB Observations from a 16-month field study using two vertically pointing radars and a disdrometer at Wallops Island are analyzed to examine the consistency of the multi-instrument observations with respect to reflectivity and Z-R relations. The vertically pointing radars were operated at S and K bands and had a very good agreement in reflectivity at a gate centered on 175 and 177 m above ground level over a variety of storms. This agreement occurred even though the sampling volumes were of different size and even though the S band measured the reflectivity factor directly, whereas the K-band radar deduced it from attenuated K-band measurements. Indeed, the radar agreement in reflectivity at the collocated range gates was superior to that between the disdrometer and either radar. This is attributed in large part to the spatial separation of the disdrometer and radar sample volumes, although the lesser agreement observed in a prior collocated disdrometer-disdrometer comparison suggests the larger size of the radar sample volumes as well as the better overlap also play a role. Vertical variations in the observations were examined with the aid of the two radar profilers. As expected, the agreement between the disdrometer reflectivity and the reflectivity seen in the vertically pointing radars decreased with height. The effect of these vertical variations on determinations of Z-R relation coefficients was then examined, using a number of different methods for finding the best fitting coefficients. The coefficient of the Z-R relation derived from paired disdrometer rain rate and radar reflectivity decreased with height, while the exponent of the Z-R relation increased with height. The coefficient and exponent of the Z-R relations also showed sensitivity to the choice of derivation method [linear and nonlinear least squares, fixed exponent, minimizing the root-mean-square difference (RMSD), and probability matching]. The influence of the time lag between the radar and disdrometer measurements was explored by examining the RMSD in reflectivity for paired measurements between 0- and 4-min lag. The no-lag conditions had the lowest RMSD up to 400 m, while 1-min lag gave the lowest RMSD at higher heights. The coefficient and exponent of the Z-R relations, on the other hand, did not have a significant change between no-lag-and 1-min-lag-based pairs. C1 [Tokay, Ali] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Tokay, Ali] Univ Maryland Baltimore Cty, Joint Ctr Earth Syst Technol, Baltimore, MD 21228 USA. [Hartmann, Peter; Battaglia, Alessandro] Univ Bonn, Inst Meteorol, D-5300 Bonn, Germany. [Gage, Kenneth S.; Clark, Wallace L.; Williams, Christopher R.] NOAA, Earth Syst Res Lab, Boulder, CO USA. [Gage, Kenneth S.; Clark, Wallace L.; Williams, Christopher R.] Univ Colorado, Cooperat Inst Res Environm Sci, Boulder, CO 80309 USA. RP Tokay, A (reprint author), NASA, Goddard Space Flight Ctr, Code 613-1, Greenbelt, MD 20771 USA. EM ali.tokay-1@nasa.gov RI Williams, Christopher/A-2723-2015 OI Williams, Christopher/0000-0001-9394-8850 NR 29 TC 24 Z9 26 U1 0 U2 4 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 JUN PY 2009 VL 26 IS 6 BP 1120 EP 1134 DI 10.1175/2008JTECHA1163.1 PG 15 WC Engineering, Ocean; Meteorology & Atmospheric Sciences SC Engineering; Meteorology & Atmospheric Sciences GA 462RB UT WOS:000267372200007 ER PT J AU Gopalswamy, N Akiyama, S Yashiro, S Michalek, G Lepping, RP AF Gopalswamy, N. Akiyama, S. Yashiro, S. Michalek, G. Lepping, R. P. TI Solar sources and geospace consequences of interplanetary magnetic clouds observed during solar cycle 23-Paper 1 (vol 70, pg 245, 2008) SO JOURNAL OF ATMOSPHERIC AND SOLAR-TERRESTRIAL PHYSICS LA English DT Correction C1 [Gopalswamy, N.; Akiyama, S.; Yashiro, S.; Michalek, G.; Lepping, R. P.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Akiyama, S.; Yashiro, S.; Michalek, G.] Catholic Univ Amer, Washington, DC 20064 USA. RP Gopalswamy, N (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. EM nat.gopalswamy@nasa.gov RI Gopalswamy, Nat/D-3659-2012 NR 1 TC 3 Z9 3 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 JUN PY 2009 VL 71 IS 8-9 BP 1005 EP 1009 DI 10.1016/j.jastp.2008.10.016 PG 5 WC Geochemistry & Geophysics; Meteorology & Atmospheric Sciences SC Geochemistry & Geophysics; Meteorology & Atmospheric Sciences GA 465HE UT WOS:000267572600027 ER PT J AU Kwon, O Tranter, M Jones, WK Sankovic, JM Banerjee, RK AF Kwon, Ohwon Tranter, Michael Jones, W. Keith Sankovic, John M. Banerjee, Rupak K. TI Differential Translocation of Nuclear Factor-KappaB in a Cardiac Muscle Cell Line Under Gravitational Changes SO JOURNAL OF BIOMECHANICAL ENGINEERING-TRANSACTIONS OF THE ASME LA English DT Article; Proceedings Paper CT 9th Annual Conference on Arteriosclerosis, Thrombosis and Vascular Biology CY APR 16-18, 2008 CL Atlanta, GA DE biomechanics; cardiology; cellular biophysics; enzymes; genetics; molecular biophysics; muscle; zero gravity experiments ID MICROGRAVITY; ACTIVATION; EXPRESSION; STRESS; HEART AB Microgravity (micro-g) environments have been shown to elicit dysregulation of specific genes in a wide assay of cell types. It is known that the activation of transcription factors and molecular signaling pathways influence various physiological outcomes associated with stress and adaptive responses. Nuclear factor-kappa B (NF-kappa B) is one of the most prevailing oxidation-sensitive transcription factors. It is hypothesized that simulated microgravity would activate NF-kappa B and its downstream transcriptional networks, thus suggesting a role for NF-kappa B in microgravity induced muscle atrophy. To investigate the activation of NF-kappa B in a rat cardiac cell line (H9c2) under micro-g, rotating wall vessel bioreactors were used to simulate micro-g conditions. Western blotting revealed that mean nuclear translocation of NF-kappa B p65 subunit was 69% for micro-g and 46% for unit-g dynamic control as compared with a 30 min TNF-alpha positive control (p < 0.05, n=3). The results from western blots were confirmed by enzyme-linked immunosorbent assay, which showed 66% for micro-g and 45% for dynamic control as compared with positive control (p < 0.05, n=3). These results show significant differential translocation of NF-kappa B p65 under simulated micro-g. These results may be expanded upon to explain physiological changes such as muscle atrophy and further identify the regulatory pathways and effector molecules activated under exposure to micro-g. C1 [Kwon, Ohwon; Banerjee, Rupak K.] Univ Cincinnati, Dept Mech Engn, Cincinnati, OH 45221 USA. [Tranter, Michael; Jones, W. Keith] Univ Cincinnati, Dept Pharmacol & Cell Biophys, Cincinnati, OH 45221 USA. [Sankovic, John M.] NASA Glenn Res Ctr, Micrograv Sci Div, Cleveland, OH 44135 USA. [Banerjee, Rupak K.] Univ Cincinnati, Dept Mech Engn, Cincinnati, OH 45221 USA. [Banerjee, Rupak K.] Univ Cincinnati, Dept Biomed Engn, Cincinnati, OH 45221 USA. RP Banerjee, RK (reprint author), Univ Cincinnati, Dept Mech Engn, Cincinnati, OH 45221 USA. EM rupak.banerjee@uc.edu OI Tranter, Michael/0000-0002-0609-3717 FU NHLBI NIH HHS [R01 HL063034] NR 24 TC 4 Z9 5 U1 0 U2 2 PU ASME-AMER SOC MECHANICAL ENG PI NEW YORK PA THREE PARK AVE, NEW YORK, NY 10016-5990 USA SN 0148-0731 J9 J BIOMECH ENG-T ASME JI J. Biomech. Eng.-Trans. ASME PD JUN PY 2009 VL 131 IS 6 AR 064503 DI 10.1115/1.3128718 PG 4 WC Biophysics; Engineering, Biomedical SC Biophysics; Engineering GA 445FO UT WOS:000266035700019 PM 19449973 ER PT J AU Yang, SC Keppenne, C Rienecker, M Kalnay, E AF Yang, Shu-Chih Keppenne, Christian Rienecker, Michele Kalnay, Eugenia TI Application of Coupled Bred Vectors to Seasonal-to-Interannual Forecasting and Ocean Data Assimilation SO JOURNAL OF CLIMATE LA English DT Article ID GENERAL-CIRCULATION MODEL; ENSEMBLE KALMAN FILTER; TROPICAL PACIFIC-OCEAN; ANALYSIS SCHEMES; EL-NINO; PART I; SALINITY; ERROR; TEMPERATURE; PROPAGATION AB Coupled bred vectors (BVs) generated from the NASA Global Modeling and Assimilation Office (GMAO) coupled general circulation model are designed to capture the uncertainties related to slowly varying coupled instabilities. Two applications of the BVs are investigated in this study. First, the coupled BVs are used as initial perturbations for ensemble-forecasting purposes. Results show that the seasonal-to-interannual variability forecast skill can be improved when the oceanic and atmospheric perturbations are initialized with coupled BVs. The impact is particularly significant when the forecasts are initialized from the cold phase of tropical Pacific SST (e. g., August and November), because at these times the early coupled model errors, not accounted for in the BVs, are small. Second, the structure of the BVs is applied to construct hybrid background error covariances carrying flow-dependent information for the ocean data assimilation. Results show that the accuracy of the ocean analyses is improved when Gaussian background covariances are supplemented with a term obtained from the BVs. The improvement is especially noticeable for the salinity field. C1 [Yang, Shu-Chih; Rienecker, Michele] NASA, Goddard Space Flight Ctr, Global Modeling & Assimilat Off, Greenbelt, MD 20771 USA. [Yang, Shu-Chih] Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20742 USA. [Yang, Shu-Chih; Kalnay, Eugenia] Univ Maryland, Dept Atmospher & Ocean Sci, College Pk, MD 20742 USA. [Keppenne, Christian] Sci Applicat Int Corp, Greenbelt, MD USA. RP Yang, SC (reprint author), Natl Cent Univ, Dept Atmospher Sci, Jhongli 32001, Taiwan. EM shuchih.yang@atm.ncu.edu.tw RI Kalnay, Eugenia/F-4393-2010; OI Kalnay, Eugenia/0000-0002-9984-9906 FU NASA [WBS 802678.02.12, NNG06GB77G] FX The authors are very grateful for technical support from the NASA GMAO staff. This research was supported by funding (WBS 802678.02.12) from NASA's Modeling, Analysis and Prediction (MAP) program. S.-C. Yang and E. Kalnay were also supported by NASA Grant NNG06GB77G. Computational resources were provided by the NASA Center for Computational Sciences at the Goddard Space Flight Center. NR 32 TC 17 Z9 18 U1 1 U2 7 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 JUN PY 2009 VL 22 IS 11 BP 2850 EP 2870 DI 10.1175/2008JCLI2427.1 PG 21 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 467SR UT WOS:000267763200004 ER PT J AU Waliser, D Sperber, K Hendon, H Kim, D Wheeler, M Weickmann, K Zhang, C Donner, L Gottschalck, J Higgins, W Kang, IS Legler, D Moncrieff, M Vitart, F Wang, B Wang, W Woolnough, S Maloney, E Schubert, S Stern, W AF Waliser, D. Sperber, K. Hendon, H. Kim, D. Wheeler, M. Weickmann, K. Zhang, C. Donner, L. Gottschalck, J. Higgins, W. Kang, I. -S. Legler, D. Moncrieff, M. Vitart, F. Wang, B. Wang, W. Woolnough, S. Maloney, E. Schubert, S. Stern, W. CA Clivar Madden-Julian Oscillation TI MJO Simulation Diagnostics SO JOURNAL OF CLIMATE LA English DT Review ID MADDEN-JULIAN OSCILLATION; TROPICAL INTRASEASONAL OSCILLATION; SEA-SURFACE TEMPERATURE; GENERAL-CIRCULATION MODEL; ASIAN SUMMER MONSOON; EXTREME PRECIPITATION EVENTS; NINO SOUTHERN-OSCILLATION; COUPLED EQUATORIAL WAVES; EASTERN NORTH PACIFIC; 30-50 DAY VARIABILITY AB The Madden-Julian oscillation (MJO) interacts with and influences a wide range of weather and climate phenomena (e. g., monsoons, ENSO, tropical storms, midlatitude weather), and represents an important, and as yet unexploited, source of predictability at the subseasonal time scale. Despite the important role of the MJO in climate and weather systems, current global circulation models (GCMs) exhibit considerable shortcomings in representing this phenomenon. These shortcomings have been documented in a number of multimodel comparison studies over the last decade. However, diagnosis of model performance has been challenging, and model progress has been difficult to track, because of the lack of a coherent and standardized set of MJO diagnostics. One of the chief objectives of the U. S. Climate Variability and Predictability (CLIVAR) MJO Working Group is the development of observation-based diagnostics for objectively evaluating global model simulations of the MJO in a consistent framework. Motivation for this activity is reviewed, and the intent and justification for a set of diagnostics is provided, along with specification for their calculation, and illustrations of their application. The diagnostics range from relatively simple analyses of variance and correlation to more sophisticated space-time spectral and empirical orthogonal function analyses. These diagnostic techniques are used to detect MJO signals, to construct composite life cycles, to identify associations of MJO activity with the mean state, and to describe interannual variability of the MJO. C1 [Waliser, D.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Sperber, K.] Lawrence Livermore Natl Lab, PCMDI, Livermore, CA USA. [Hendon, H.; Wheeler, M.] Ctr Australian Weather & Climate Res, Melbourne, Vic, Australia. [Kim, D.] Seoul Natl Univ, Seoul, South Korea. [Maloney, E.] Colorado State Univ, Ft Collins, CO 80523 USA. [Weickmann, K.] NOAA Earth Syst Res Lab, Boulder, CO USA. [Zhang, C.] Univ Miami, Rosenstiel Sch Marine & Atmospher Sci, Miami, FL 33149 USA. [Donner, L.; Stern, W.] NOAA GFDL, Princeton, NJ USA. [Gottschalck, J.; Higgins, W.; Wang, W.] NOAA NCEP, Camp Springs, MD USA. [Kang, I. -S.] Seoul Natl Univ, Seoul, South Korea. [Legler, D.] US CLIVAR Off, Washington, DC USA. [Moncrieff, M.] NCAR, Boulder, CO USA. [Schubert, S.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Vitart, F.] European Ctr Medium Range Weather Forecasts, Reading RG2 9AX, Berks, England. [Wang, B.] Univ Hawaii Manoa, IPRC, Honolulu, HI 96822 USA. [Woolnough, S.] Univ Reading, Reading, Berks, England. RP Waliser, D (reprint author), CALTECH, Jet Prop Lab, MS 183-505,4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM duane.waliser@jpl.nasa.gov RI Wheeler, Matthew/C-9038-2011; Maloney, Eric/A-9327-2008; Sperber, Kenneth/H-2333-2012; 안, 민섭/D-9972-2015 OI Wheeler, Matthew/0000-0002-9769-1973; Maloney, Eric/0000-0002-2660-2611; FU U.S. CLIVAR and International CLIVAR; U.S. Department of Energy Office of Science; Lawrence Livermore National Laboratory [DE-AC52-07NA27344]; NSF Climate and Large-Scale Dynamics Program [ATM-063234]; NOAA CPPA Award [NA05OAR4310006]; NSF [ATM0739402]; NOAA Office of Global Programs through the Cooperative Institute for Marine and Atmospheric Studies (CIMAS); Korea Meteorological Administration Research and Development Program [CATER_ 2006-4206]; BK21 program FX The MJOWG wishes to acknowledge and thank U.S. CLIVAR and International CLIVAR for supporting this working group and its activities. We would like to specifically acknowledge the administrative support on behalf of the MJOWG by Cathy Stevens of the U.S. CLIVAR Office. KRS was supported under the auspices of the U.S. Department of Energy Office of Science, Climate Change Prediction Program by Lawrence Livermore National Laboratory under Contract DE-AC52-07NA27344. DEW's contributions to this study were carried out on behalf of the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration (NASA). EDM was supported by the NSF Climate and Large-Scale Dynamics Program under Grant ATM-063234, and by NOAA CPPA Award NA05OAR4310006. CZ was support by NSF Grant ATM0739402 and by the NOAA Office of Global Programs through the Cooperative Institute for Marine and Atmospheric Studies (CIMAS). D. Kim and I. Kang were supported by the Korea Meteorological Administration Research and Development Program under Grant CATER_ 2006-4206 and BK21 program. NR 138 TC 110 Z9 111 U1 1 U2 25 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 JUN PY 2009 VL 22 IS 11 BP 3006 EP 3030 DI 10.1175/2008JCLI2731.1 PG 25 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 467SR UT WOS:000267763200013 ER PT J AU Findell, KL Pitman, AJ England, MH Pegion, PJ AF Findell, Kirsten L. Pitman, Andrew J. England, Matthew H. Pegion, Philip J. TI Regional and Global Impacts of Land Cover Change and Sea Surface Temperature Anomalies SO JOURNAL OF CLIMATE LA English DT Article ID TROPICAL DEFORESTATION; PART I; CARBON-DIOXIDE; CLIMATE MODEL; ATMOSPHERE; PRECIPITATION; CIRCULATION; VEGETATION; PARAMETERIZATION; SENSITIVITY AB The atmospheric and land components of the Geophysical Fluid Dynamics Laboratory's (GFDL's) Climate Model version 2.1 (CM2.1) is used with climatological sea surface temperatures (SSTs) to investigate the relative climatic impacts of historical anthropogenic land cover change (LCC) and realistic SST anomalies. The SST forcing anomalies used are analogous to signals induced by El Nino-Southern Oscillation (ENSO), the North Atlantic Oscillation (NAO), and the background global warming trend. Coherent areas of LCC are represented throughout much of central and eastern Europe, northern India, southeastern China, and on either side of the ridge of the Appalachian Mountains in North America. Smaller areas of change are present in various tropical regions. The land cover changes in the model are almost exclusively a conversion of forests to grasslands. Model results show that, at the global scale, the physical impacts of LCC on temperature and rainfall are less important than large-scale SST anomalies, particularly those due to ENSO. However, in the regions where the land surface has been altered, the impact of LCC can be equally or more important than the SST forcing patterns in determining the seasonal cycle of the surface water and energy balance. Thus, this work provides a context for the impacts of LCC on climate: namely, strong regional-scale impacts that can significantly change globally averaged fields but that rarely propagate beyond the disturbed regions. This suggests that proper representation of land cover conditions is essential in the design of climate model experiments, particularly if results are to be used for regional-scale assessments of climate change impacts. C1 [Findell, Kirsten L.] NOAA, Geophys Fluid Dynam Lab, Princeton, NJ 08540 USA. [Findell, Kirsten L.; Pitman, Andrew J.; England, Matthew H.] Univ New S Wales, Climate Change Res Ctr, Sydney, NSW, Australia. [Pegion, Philip J.] NASA, Goddard Space Flight Ctr, Global Modeling & Assimilat Off, Greenbelt, MD 20771 USA. [Pegion, Philip J.] Sci Applicat Int Corp, Beltsville, MD USA. RP Findell, KL (reprint author), NOAA, Geophys Fluid Dynam Lab, 201 Forrestal Rd, Princeton, NJ 08540 USA. EM kirsten.findell@noaa.gov RI Pitman, Andrew/A-7353-2011; Pegion, Philip/E-5247-2012; England, Matthew/A-7539-2011; Findell, Kirsten/D-4430-2014 OI Pitman, Andrew/0000-0003-0604-3274; England, Matthew/0000-0001-9696-2930; NR 61 TC 34 Z9 37 U1 5 U2 34 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 JUN PY 2009 VL 22 IS 12 BP 3248 EP 3269 DI 10.1175/2008JCLI2580.1 PG 22 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 472JI UT WOS:000268126300005 ER PT J AU Koster, RD Schubert, SD Suarez, MJ AF Koster, R. D. Schubert, S. D. Suarez, M. J. TI Analyzing the Concurrence of Meteorological Droughts and Warm Periods, with Implications for the Determination of Evaporative Regime SO JOURNAL OF CLIMATE LA English DT Article ID CONTIGUOUS UNITED-STATES; SOIL-MOISTURE; PRECIPITATION; TEMPERATURE; CLIMATE; CIRCULATION; SURFACE; MODELS AB The hydroclimatic conditions under which a seasonal meteorological drought (below-normal seasonal rainfall) can induce an increase in seasonal air temperature are investigated, first with an atmospheric general circulation model (AGCM) and then with observations. Geographical differences in the dryness-warmth connection abound in the AGCM; in the United States, for example, identified evaporative controls tend to tie meteorological droughts to warmer temperatures in the South but not in the Northeast. The strong agreement between AGCM and observations-based geographical patterns of drought-induced warming supports the idea that the same evaporative controls are also present in nature. A powerful side benefit of the analysis of drought-induced warming is a Northern Hemisphere map, derived solely from observations, showing where total boreal summer evaporation is controlled by soil moisture, energy availability, or both. C1 [Koster, R. D.; Schubert, S. D.; Suarez, M. J.] NASA, Goddard Space Flight Ctr, GMAO, Greenbelt, MD 20771 USA. RP Koster, RD (reprint author), NASA, Goddard Space Flight Ctr, GMAO, Code 610 1, Greenbelt, MD 20771 USA. EM randal.d.koster@nasa.gov RI Koster, Randal/F-5881-2012 OI Koster, Randal/0000-0001-6418-6383 NR 22 TC 46 Z9 46 U1 1 U2 21 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 JUN PY 2009 VL 22 IS 12 BP 3331 EP 3341 DI 10.1175/2008JCLI2718.1 PG 11 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 472JI UT WOS:000268126300010 ER PT J AU Stelian, C Volz, MP Derby, JJ AF Stelian, Carmen Volz, Martin P. Derby, Jeffrey J. TI On favorable thermal fields for detached Bridgman growth SO JOURNAL OF CRYSTAL GROWTH LA English DT Article DE Computer simulation; Heat transfer; Bridgman technique; Growth from melt ID CZOCHRALSKI CRYSTAL-GROWTH; GERMANIUM-CRYSTALS; SOLIDIFICATION; MICROGRAVITY; GRAVITY; MODEL; SHAPE AB The thermal fields of two Bridgman-like configurations, representative of real systems used in prior experiments for the detached growth of CdTe and Ge crystals, are studied. These detailed heat transfer computations are performed using the CrysMAS code and expand upon our previous analysis [C. Stelian, A. Yeckel, J.J. Derby, Influence of thermal phenomena on crystal reattachment during the dewetted Bridgman growth, J. Cryst. Growth, in press] that posited a new mechanism involving the thermal field and meniscus position to explain stable conditions for dewetted Bridgman growth. Computational results indicate that heat transfer conditions that led to successful detached growth in both of these systems are in accordance with our prior assertion, namely that the prevention of crystal reattachment to the crucible wall requires the avoidance of any undercooling of the melt meniscus during the growth run. Significantly, relatively simple process modifications that promote favorable thermal conditions for detached growth may overcome detrimental factors associated with meniscus shape and crucible wetting. Thus, these ideas may be important to advance the practice of detached growth for many materials. (C) 2009 Elsevier B.V. All rights reserved. C1 [Derby, Jeffrey J.] Univ Minnesota, Dept Chem Engn & Mat Sci, Minneapolis, MN 55455 USA. [Stelian, Carmen] W Univ Timisoara, Dept Phys, Timisoara 300223, Romania. [Volz, Martin P.] NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA. RP Derby, JJ (reprint author), Univ Minnesota, Dept Chem Engn & Mat Sci, 421 Washington Ave SE, Minneapolis, MN 55455 USA. EM derby@umn.edu OI Derby, Jeffrey/0000-0001-6418-2155 FU National Nuclear Security Administration [DE-FG52-06NA27498] FX This work has been supported in part by the Minnesota Supercomputing Institute and the Department of Energy, National Nuclear Security Administration, under Award number DE-FG52-06NA27498, the content of which does not necessarily reflect the position or policy of the United States Government, and no official endorsement should be inferred. C.S. acknowledges support from the Alexander Dubcek Fund, administered by the Office of International Programs of the University of Minnesota. J.J.D. wishes to thank J. Friedrich, T. Jung, and G. Ardelean of the Crystal Growth Laboratory, Fraunhofer IISB, for ongoing collaborations involving CrysMAS. NR 25 TC 9 Z9 10 U1 0 U2 4 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 JUN 1 PY 2009 VL 311 IS 12 BP 3337 EP 3346 DI 10.1016/j.jcrysgro.2009.03.043 PG 10 WC Crystallography; Materials Science, Multidisciplinary; Physics, Applied SC Crystallography; Materials Science; Physics GA 467UM UT WOS:000267768600020 ER PT J AU Nguyen, NT AF Nguyen, Nhan T. TI One-Dimensional Unsteady Periodic Flow Model with Boundary Conditions Constrained by Differential Equations SO JOURNAL OF FLUIDS ENGINEERING-TRANSACTIONS OF THE ASME LA English DT Article DE confined flow; differential equations; finite difference methods; transonic flow AB This paper describes a modeling method for closed-loop unsteady fluid transport systems based on 1D unsteady Euler equations with nonlinear forced periodic boundary conditions. A significant feature of this model is the incorporation of dynamic constraints on the variables that control the transport process at the system boundaries as they often exist in many transport systems. These constraints result in a coupling of the Euler equations with a system of ordinary differential equations that model the dynamics of auxiliary processes connected to the transport system. Another important feature of the transport model is the use of a quasilinear form instead of the flux-conserved form. This form lends itself to modeling with measurable conserved fluid transport variables and represents an intermediate model between the primitive variable approach and the conserved variable approach. A wave-splitting finite-difference upwind method is presented as a numerical solution of the model. An iterative procedure is implemented to solve the nonlinear forced periodic boundary conditions prior to the time-marching procedure for the upwind method. A shock fitting method to handle transonic flow for the quasilinear form of the Euler equations is presented. A closed-loop wind tunnel is used for demonstration of the accuracy of this modeling method. C1 NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Nguyen, NT (reprint author), NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. NR 19 TC 1 Z9 1 U1 0 U2 1 PU ASME-AMER SOC MECHANICAL ENG PI NEW YORK PA THREE PARK AVE, NEW YORK, NY 10016-5990 USA SN 0098-2202 J9 J FLUID ENG-T ASME JI J. Fluids Eng.-Trans. ASME PD JUN PY 2009 VL 131 IS 6 AR 061201 DI 10.1115/1.3130244 PG 15 WC Engineering, Mechanical SC Engineering GA 464MB UT WOS:000267508000005 ER PT J AU Wiese, DN Folkner, WM Nerem, RS AF Wiese, D. N. Folkner, W. M. Nerem, R. S. TI Alternative mission architectures for a gravity recovery satellite mission SO JOURNAL OF GEODESY LA English DT Article DE GRACE; Cartwheel orbits; Temporal gravity; Aliasing; GRACE follow-on mission AB Since its launch in 2002, the Gravity Recovery and Climate Experiment (GRACE) mission has been providing measurements of the time-varying Earth gravity field. The GRACE mission architecture includes two satellites in near-circular, near-polar orbits separated in the along-track direction by approximately 220 km (e.g. collinear). A microwave ranging instrument measures changes in the distance between the spacecraft, while accelerometers on each spacecraft are used to measure changes in distance due to non-gravitational forces. The fact that the satellites are in near-polar orbits coupled with the fact that the inter-satellite range measurements are directed in the along-track direction, contributes to longitudinal striping in the estimated gravity fields. This paper examines four candidate mission architectures for a future gravity recovery satellite mission to assess their potential in measuring the gravity field more accurately than GRACE. All satellites were assumed to have an improved measurement system, with an inter-satellite laser ranging instrument and a drag-free system for removal of non-gravitational accelerations. Four formations were studied: a two-satellite collinear pair similar to GRACE; a four-satellite architecture with two collinear pairs; a two-satellite cartwheel formation; and a four-satellite cartwheel formation. A cartwheel formation consists of satellites performing in-plane, relative elliptical motion about their geometric center, so that inter-satellite measurements are, at times, directed radially (e.g. parallel to the direction towards the center of the Earth) rather than along-track. Radial measurements, unlike along-track measurements, have equal sensitivity to mass distribution in all directions along the Earth's surface and can lead to higher spatial resolution in the derived gravity field. The ability of each architecture to recover the gravity field was evaluated using numerical simulations performed with JPL's GIPSY-OASIS software package. Thirty days of data were used to estimate gravity fields complete to degree and order 60. Evaluations were done for 250 and 400 km nominal orbit altitudes. The sensitivity of the recovered gravity field to under-sampled effects was assessed using simulated errors in atmospheric/ocean dealiasing (AOD) models. Results showed the gravity field errors associated with the four-satellite cartwheel formation were approximately one order of magnitude lower than the collinear satellite pair when only measurement system errors were included. When short-period AOD model errors were introduced, the gravity field errors for each formation were approximately the same. The cartwheel formations eliminated most of the longitudinal striping seen in the gravity field errors. A covariance analysis showed the error spectrum of the cartwheel formations to be lower and more isotropic than that of the collinear formations. C1 [Wiese, D. N.; Nerem, R. S.] Univ Colorado, Colorado Ctr Astrodynam Res, Boulder, CO 80309 USA. [Folkner, W. M.] CALTECH, Jet Prop Lab, Pasadena, CA 91101 USA. RP Wiese, DN (reprint author), Univ Colorado, Colorado Ctr Astrodynam Res, 431 UCB, Boulder, CO 80309 USA. EM wiese@colorado.edu; William.M.Folkner@jpl.nasa.gov; nerem@colorado.edu FU National Defense Science and Engineering Graduate Fellowship program; National Aeronautics and Space Administration FX This research was funded by the Department of Defense through the National Defense Science and Engineering Graduate Fellowship program. It was also partially funded by the National Aeronautics and Space Administration Instrument Incubator Program (IIP) through the Earth Science Technology Office. A special thanks goes to Dr. Willy Bertiger of Jet Propulsion Laboratory (JPL) for his help with GIPSY and Dr. Paul Thompson of JPL for providing the Atmosphere and Ocean Dealiasing (AOD) error models. Finally, I would like to thank Dr. Mike Watkins of JPL for supporting my time spent at JPL on this project in the summer of 2006. The research described in this paper was in part carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. The authors would also like to thank an editor of the Journal of Geodesy, Pavel Ditmar, along with four anonymous reviewers for constructive feedback and suggestions on this paper. NR 21 TC 31 Z9 39 U1 0 U2 13 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0949-7714 EI 1432-1394 J9 J GEODESY JI J. Geodesy PD JUN PY 2009 VL 83 IS 6 BP 569 EP 581 DI 10.1007/s00190-008-0274-1 PG 13 WC Geochemistry & Geophysics; Remote Sensing SC Geochemistry & Geophysics; Remote Sensing GA 448FV UT WOS:000266249400007 ER PT J AU Santanello, JA Peters-Lidard, CD Kumar, SV Alonge, C Tao, WK AF Santanello, Joseph A., Jr. Peters-Lidard, Christa D. Kumar, Sujay V. Alonge, Charles Tao, Wei-Kuo TI A Modeling and Observational Framework for Diagnosing Local Land-Atmosphere Coupling on Diurnal Time Scales SO JOURNAL OF HYDROMETEOROLOGY LA English DT Article ID BOUNDARY-LAYER INTERACTIONS; SURFACE PARAMETERIZATION SCHEMES; HETEROGENEOUS SOIL-MOISTURE; GENERAL-CIRCULATION MODELS; SOUTHERN GREAT-PLAINS; MESOSCALE ETA-MODEL; VERTICAL DIFFUSION; FORECAST MODEL; BUDGET METHODS; MIXED-LAYER AB Land-atmosphere interactions play a critical role in determining the diurnal evolution of both planetary boundary layer (PBL) and land surface temperature and moisture states. The degree of coupling between the land surface and PBL in numerical weather prediction and climate models remains largely unexplored and undiagnosed because of the complex interactions and feedbacks present across a range of scales. Furthermore, uncoupled systems or experiments [e. g., the Project for the Intercomparison of Land-Surface Parameterization Schemes (PILPS)] may lead to inaccurate water and energy cycle process understanding by neglecting feedback processes such as PBL-top entrainment. In this study, a framework for diagnosing local land-atmosphere coupling is presented using a coupled mesoscale model with a suite of PBL and land surface model (LSM) options along with observations during field experiments in the U. S. Southern Great Plains. Specifically, the Weather Research and Forecasting Model (WRF) has been coupled to the Land Information System (LIS), which provides a flexible and high-resolution representation and initialization of land surface physics and states. Within this framework, the coupling established by each pairing of the available PBL schemes in WRF with the LSMs in LIS is evaluated in terms of the diurnal temperature and humidity evolution in the mixed layer. The coevolution of these variables and the convective PBL are sensitive to and, in fact, integrative of the dominant processes that govern the PBL budget, which are synthesized through the use of mixing diagrams. Results show how the sensitivity of land-atmosphere interactions to the specific choice of PBL scheme and LSM varies across surface moisture regimes and can be quantified and evaluated against observations. As such, this methodology provides a potential pathway to study factors controlling local land-atmosphere coupling (LoCo) using the LIS-WRF system, which will serve as a test bed for future experiments to evaluate coupling diagnostics within the community. C1 [Santanello, Joseph A., Jr.; Peters-Lidard, Christa D.; Kumar, Sujay V.; Alonge, Charles] NASA, Goddard Space Flight Ctr, Hydrol Sci Branch, Greenbelt, MD 20771 USA. [Kumar, Sujay V.] Univ Maryland, Goddard Earth Sci & Technol Ctr, Baltimore, MD 21201 USA. [Kumar, Sujay V.; Alonge, Charles] Sci Applicat Int Corp, Beltsville, MD USA. [Tao, Wei-Kuo] NASA, Goddard Space Flight Ctr, Mesoscale Proc Branch, Greenbelt, MD 20771 USA. RP Santanello, JA (reprint author), NASA, Goddard Space Flight Ctr, Hydrol Sci Branch, GSFC Code 614-3,Bldg 22,Room 008, Greenbelt, MD 20771 USA. EM joseph.a.santanello@nasa.gov RI Santanello, Joseph/D-4438-2012; Kumar, Sujay/B-8142-2015; Peters-Lidard, Christa/E-1429-2012 OI Santanello, Joseph/0000-0002-0807-6590; Peters-Lidard, Christa/0000-0003-1255-2876 FU NASA FX This work was supported by the NASA Energy and Water Cycle Study (NEWS; principal investiagor Peters-Lidard). We thank NEWS, ESSIC, and GSFC for helping to make the completion of this work possible. In particular, Jim Geiger and Joe Eastman were instrumental in providing feedback and activities related to LIS-WRF. We also appreciate the past and ongoing collaboration with the LoCo community that has stimulated this work, in particular Bert Holtslag, Bart van den Hurk, Paul Houser, and Dara Entekhabi. NR 79 TC 87 Z9 87 U1 5 U2 17 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 1525-755X J9 J HYDROMETEOROL JI J. Hydrometeorol. PD JUN PY 2009 VL 10 IS 3 BP 577 EP 599 DI 10.1175/2009JHM1066.1 PG 23 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 463HB UT WOS:000267420900001 ER PT J AU Nourbakhsh, A Chaljub, G Garges, KJ AF Nourbakhsh, Ali Chaljub, Gregory Garges, Kim J. TI SPONTANEOUS CERVICAL EPIDURAL HEMATOMA MASQUERADING AS AN ABSCESS ON MAGNETIC RESONANCE IMAGING SCAN SO JOURNAL OF MANIPULATIVE AND PHYSIOLOGICAL THERAPEUTICS LA English DT Article DE Hematoma; Epidural; Spinal; Neck Abscess ID CONTRAST ENHANCEMENT; SURGICAL-MANAGEMENT; ETIOLOGY; PARAPLEGIA; RESOLUTION AB Objective: The aims of the study are to describe a case of spontaneous spinal epidural hematoma (SSEH) without any predisposing factors and magnetic resonance imaging (MRI) features of epidural abscess and to highlight the importance of high clinical suspicion. Clinical Features: A 75-year-old male presented to the emergency department after a severe neck pain. He progressively showed sensory and upper motor signs on the left side of the body. The MRI scans were suggestive of cervical epidural abscess with peripheral enhancement of the lesion. Interventions and Outcomes: He underwent a multiple level (C3-T1) laminectomy when he was found to have an SSEH. There has been no history of trauma or other predisposing factor, and presence of arteriovenous malformation was ruled out by MR angiography. Conclusions: The MRI features of SSEH may be misleading and mimic other spinal lesions such as abscess. Presence of tapering superior and inferior margins, spotty Gadolinium enhancement in the mass, along with abrupt clinical onset of pain and neurologic deficit, should raise the suspicion toward epidural hematoma. Enhancement in the hyperacute stage of the hematoma itself might indicate continued bleeding and, in the case of deteriorating neurologic status, will necessitate decompression. (J Manipulative Physiol Ther 2009-132:391-395) C1 [Nourbakhsh, Ali; Garges, Kim J.] Univ Texas Med Branch, Dept Orthoped Surg & Rehabil, Div Spine Surg, Galveston, TX USA. [Chaljub, Gregory] Univ Texas Med Branch, Dept Radiol, Galveston, TX USA. RP Garges, KJ (reprint author), NASA, Spine Inst, 18100 St John Dr, Houston, TX 77058 USA. EM kjgarges@earthlink.net NR 19 TC 2 Z9 2 U1 0 U2 1 PU MOSBY-ELSEVIER PI NEW YORK PA 360 PARK AVENUE SOUTH, NEW YORK, NY 10010-1710 USA SN 0161-4754 J9 J MANIP PHYSIOL THER JI J. Manip. Physiol. Ther. PD JUN PY 2009 VL 32 IS 5 BP 391 EP 395 DI 10.1016/j.jmpt.2009.04.007 PG 5 WC Health Care Sciences & Services; Integrative & Complementary Medicine; Rehabilitation SC Health Care Sciences & Services; Integrative & Complementary Medicine; Rehabilitation GA 462CZ UT WOS:000267324900009 PM 19539123 ER PT J AU Hatamleh, O Singh, PM Garmestani, H AF Hatamleh, Omar Singh, Preet M. Garmestani, Hamid TI Stress Corrosion Cracking Behavior of Peened Friction Stir Welded 2195 Aluminum Alloy Joints SO JOURNAL OF MATERIALS ENGINEERING AND PERFORMANCE LA English DT Article DE friction stir welding; laser peening; shot peening; stress corrosion cracking; 2195 ID RESIDUAL-STRESSES; FATIGUE; MICROSTRUCTURE; LITHIUM AB The surface treatment techniques of laser and shot peening were used to investigate their effect on stress corrosion cracking (SCC) in friction stir welded (FSW) 2195 aluminum alloy joints. The investigation consisted of two parts: the first part explored the peening effects on slow strain rate testing (SSRT) in a 3.5% NaCl solution, while the second part investigated the effects of peening on corrosion while submerged in a 3.5% NaCl solution with no external loads applied. For the SSRT, the laser-peened samples demonstrated superior properties to the other samples, but no signs of corrosion pitting or SCC were evident on any of the samples. For the second part of the study, the FSW plates were inspected periodically for signs of corrosion. After 60 days there were signs of corrosion pitting, but no stress corrosion cracking was noticed in any of the peened and unpeened samples. C1 [Hatamleh, Omar] NASA, Lyndon B Johnson Space Ctr, Struct Branch, Houston, TX 77058 USA. [Singh, Preet M.; Garmestani, Hamid] Georgia Inst Technol, Sch Mat Sci & Engn, Atlanta, GA 30332 USA. RP Hatamleh, O (reprint author), NASA, Lyndon B Johnson Space Ctr, Struct Branch, Houston, TX 77058 USA. EM omar.hatamleh-1@nasa.gov NR 25 TC 8 Z9 8 U1 4 U2 35 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 1059-9495 J9 J MATER ENG PERFORM JI J. Mater. Eng. Perform. PD JUN PY 2009 VL 18 IS 4 BP 406 EP 413 DI 10.1007/s11665-008-9303-8 PG 8 WC Materials Science, Multidisciplinary SC Materials Science GA 445GQ UT WOS:000266038900010 ER PT J AU Hatamleh, O DeWald, A AF Hatamleh, Omar DeWald, Adrian TI An investigation of the peening effects on the residual stresses in friction stir welded 2195 and 7075 aluminum alloy joints SO JOURNAL OF MATERIALS PROCESSING TECHNOLOGY LA English DT Article DE Friction stir welding; User peening; Shot peening; X-ray diffraction; Contour method; 2195; 7075 ID FATIGUE-CRACK-GROWTH; 7075-T7351 ALUMINUM; LASER AB Surface treatment processes including laser and shot peening were applied to friction stir welded samples fabricated using aluminum alloys (AA) 2195 and 7075. Surface residual stress measurements on these samples were acquired using X-ray diffraction. Measurements of the through thickness bulk residual stresses were obtained using the contour method. The deepest compressive residual stresses were obtained with multiple layers of laser peening, and increased proportionally as the number of peening layers increased for AA 2195. For AA 7075, little change was noticed in the residual stresses as the number of peening layers increased. Interestingly, laser peening was shown to have less of an effect on residual stress near the edges of the weld joint where significant softening occurred. Published by Elsevier B.V. C1 [Hatamleh, Omar] NASA, Lyndon B Johnson Space Ctr, Struct Branch, Houston, TX 77058 USA. [DeWald, Adrian] Hill Engn LLC, Mcclellan, CA 95652 USA. RP Hatamleh, O (reprint author), NASA, Lyndon B Johnson Space Ctr, Struct Branch, Houston, TX 77058 USA. EM omar.hatamleh-1@nasa.gov NR 18 TC 16 Z9 18 U1 2 U2 25 PU ELSEVIER SCIENCE SA PI LAUSANNE PA PO BOX 564, 1001 LAUSANNE, SWITZERLAND SN 0924-0136 J9 J MATER PROCESS TECH JI J. Mater. Process. Technol. PD JUN 1 PY 2009 VL 209 IS 10 BP 4822 EP 4829 DI 10.1016/j.jmatprotec.2008.12.010 PG 8 WC Engineering, Industrial; Engineering, Manufacturing; Materials Science, Multidisciplinary SC Engineering; Materials Science GA 467WX UT WOS:000267774900029 ER PT J AU Rothman, LS Brown, LR Vander Auwera, J AF Rothman, Laurence S. Brown, Linda R. Vander Auwera, Jean TI SPECIAL ISSUE HITRAN 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 02318 USA. [Brown, Linda R.] CALTECH, Jet Prop Lab, Div Sci, Pasadena, CA 91109 USA. [Vander Auwera, Jean] Univ Libre Bruxelles, FRS FNRS, Serv Chim Quant & Photophys, B-1050 Brussels, Belgium. RP Rothman, LS (reprint author), Harvard Smithsonian Ctr Astrophys, Atom & Mol Phys Div, 60 Garden St, Cambridge, MA 02318 USA. EM lrothman@cfa.harvard.edu OI Rothman, Laurence/0000-0002-3837-4847 NR 0 TC 0 Z9 0 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 JUN-JUL PY 2009 VL 110 IS 9-10 BP 531 EP 532 DI 10.1016/j.jqsrt.2009.02.025 PG 2 WC Optics; Spectroscopy SC Optics; Spectroscopy GA 447HD UT WOS:000266181300001 ER PT J AU Rothman, LS Gordon, IE Barbe, A Benner, DC Bernath, PE Birk, M Boudon, V Brown, LR Campargue, A Champion, JP Chance, K Coudert, LH Dana, V Devi, VM Fally, S Flaud, JM Gamache, RR Goldman, A Jacquemart, D Kleiner, I Lacome, N Lafferty, WJ Mandin, JY Massie, ST Mikhailenko, SN Miller, CE Moazzen-Ahmadi, N Naumenko, OV Nikitin, AV Orphal, J Perevalov, VI Perrin, A Predoi-Cross, A Rinsland, CP Rotger, M Simeckova, M Smith, MAH Sung, K Tashkun, SA Tennyson, J Toth, RA Vandaele, AC Vander Auwera, J AF Rothman, L. S. Gordon, I. E. Barbe, A. Benner, D. Chris Bernath, P. E. Birk, M. Boudon, V. Brown, L. R. Campargue, A. Champion, J. -P. Chance, K. Coudert, L. H. Dana, V. Devi, V. M. Fally, S. Flaud, J. -M. Gamache, R. R. Goldman, A. Jacquemart, D. Kleiner, I. Lacome, N. Lafferty, W. J. Mandin, J. -Y. Massie, S. T. Mikhailenko, S. N. Miller, C. E. Moazzen-Ahmadi, N. Naumenko, O. V. Nikitin, A. V. Orphal, J. Perevalov, V. I. Perrin, A. Predoi-Cross, A. Rinsland, C. P. Rotger, M. Simeckova, M. Smith, M. A. H. Sung, K. Tashkun, S. A. Tennyson, J. Toth, R. A. Vandaele, A. C. Vander Auwera, J. TI The HITRAN 2008 molecular spectroscopic database SO JOURNAL OF QUANTITATIVE SPECTROSCOPY & RADIATIVE TRANSFER LA English DT Review DE HITRAN; Spectroscopic database; Molecular spectroscopy; Molecular absorption; Spectroscopic line parameters; Absorption cross-sections; Aerosols ID ABSORPTION CROSS-SECTIONS; ABSOLUTE LINE-INTENSITIES; FOURIER-TRANSFORM SPECTROSCOPY; SELF-BROADENING COEFFICIENTS; DIODE-LASER MEASUREMENTS; HIGH-RESOLUTION ANALYSIS; WATER-VAPOR TRANSITIONS; OXYGEN A-BAND; MU-M REGION; CONSTRAINED MULTISPECTRUM ANALYSIS AB This paper describes the status of the 2008 edition of the HITRAN molecular spectroscopic database. The new edition is the first official public release since the 2004 edition, although a number of crucial updates had been made available online since 2004. The HITRAN compilation consists of several components that serve as input for radiative-transfer calculation codes: individual line parameters for the microwave through visible spectra of molecules in the gas phase; absorption cross-sections for molecules having dense spectral features, i.e. spectra in which the individual lines are not resolved; individual line parameters and absorption cross-sections for bands in the ultraviolet; refractive indices of aerosols, tables and files of general properties associated with the database; and database management software. The line-by-line portion of the database contains spectroscopic parameters for 42 molecules including many of their isotopologues. (c) 2009 Elsevier Ltd. All rights reserved. C1 [Rothman, L. S.; Gordon, I. E.; Chance, K.; Simeckova, M.] Harvard Smithsonian Ctr Astrophys, Atom & Mol Phys Div, Cambridge, MA 02138 USA. [Barbe, A.; Rotger, M.] Univ Reims, Grp Spectrometrie Mol & Atmospher, F-51062 Reims, France. [Benner, D. Chris; Devi, V. M.] Coll William & Mary, Dept Phys, Williamsburg, VA 23187 USA. [Bernath, P. E.] Univ York, Dept Chem, York YO10 5DD, N Yorkshire, England. [Birk, M.] DLR Remote Sensing Technol Inst, Wessling, Germany. [Boudon, V.; Champion, J. -P.; Rotger, M.] Univ Bourgogne, CNRS, Inst Carnot Bourgogne, F-21078 Dijon, France. [Brown, L. R.; Miller, C. E.; Sung, K.; Toth, R. A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Campargue, A.] Univ Grenoble 1, CNRS, Spectrometrie Phys Lab, F-38402 St Martin Dheres, France. [Dana, V.; Mandin, J. -Y.] Univ Paris 06, UPMC, UMR 7092, Lab Phys Mol & Applicat, F-75252 Paris, France. [Fally, S.] Univ Libre Bruxelles, Serv Chim Quant & Photophys, B-1050 Brussels, Belgium. [Gamache, R. R.] Univ Mass Lowell, Dept Environm Earth & Atmospher Sci, Lowell, MA 01854 USA. [Goldman, A.] Univ Denver, Dept Phys, Denver, CO 80208 USA. [Jacquemart, D.] Univ Paris 06, UPMC, UMR 7075, Lab Dynam Interact & React, F-75252 Paris, France. [Lafferty, W. J.] NIST, Gaithersburg, MD 20899 USA. [Massie, S. T.] Natl Ctr Atmospher Res, Boulder, CO 80307 USA. [Mikhailenko, S. N.; Naumenko, O. V.; Nikitin, A. V.; Perevalov, V. I.; Tashkun, S. A.] Inst Atmospher Opt, Tomsk 634055, Russia. [Moazzen-Ahmadi, N.] Univ Calgary, Dept Phys & Astron, Calgary, AB T2N 1N4, Canada. [Predoi-Cross, A.] Univ Lethbridge, Dept Phys & Astron, Lethbridge, AB T1K 3M4, Canada. [Rinsland, C. P.; Smith, M. A. H.] NASA, Langley Res Ctr, Sci Directorate, Hampton, VA 23681 USA. [Tennyson, J.] UCL, Dept Phys & Astron, London WC1E 6BT, England. [Vandaele, A. C.] Inst Aeron Spatiale Belgique, B-1180 Brussels, Belgium. RP Rothman, LS (reprint author), Harvard Smithsonian Ctr Astrophys, Atom & Mol Phys Div, 60 Garden St, Cambridge, MA 02138 USA. EM lrothman@cfa.harvard.edu RI BOUDON, Vincent/A-4504-2010; Champion, Jean-Paul/C-3963-2009; Lacome, Nelly/A-7043-2008; Bernath, Peter/B-6567-2012; Tennyson, Jonathan/I-2222-2012; Orphal, Johannes/A-8667-2012; Nikitin, Andrei/K-2624-2013; Tashkun, Sergey/E-8682-2014; Sung, Keeyoon/I-6533-2015; OI Rothman, Laurence/0000-0002-3837-4847; Gordon, Iouli/0000-0003-4763-2841; Bernath, Peter/0000-0002-1255-396X; Tennyson, Jonathan/0000-0002-4994-5238; Orphal, Johannes/0000-0002-1943-4496; Nikitin, Andrei/0000-0002-4280-4096; Chance, Kelly/0000-0002-7339-7577 NR 368 TC 2138 Z9 2222 U1 32 U2 260 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 JUN-JUL PY 2009 VL 110 IS 9-10 SI SI BP 533 EP 572 DI 10.1016/j.jqsrt.2009.02.013 PG 40 WC Optics; Spectroscopy SC Optics; Spectroscopy GA 447HD UT WOS:000266181300002 ER PT J AU Tennyson, J Bernath, PF Brown, LR Campargue, A Carleere, MR Csaszar, AG Gamache, RR Hodges, JT Jenouvrier, A Naumenko, OV Polyansky, OL Rothman, LS Toth, RA Vandaele, AC Zobov, NF Daumont, L Fazliev, AZ Furtenbacher, T Gordon, IE Mikhailenko, SN Shirin, SV AF Tennyson, Jonathan Bernath, Peter F. Brown, Linda R. Campargue, Alain Carleere, Michel R. Csaszar, Attila G. Gamache, Robert R. Hodges, Joseph T. Jenouvrier, Alain Naumenko, Olga V. Polyansky, Oleg L. Rothman, Laurence S. Toth, Robert A. Vandaele, Ann Carine Zobov, Nikolai F. Daumont, Ludovic Fazliev, Alexander Z. Furtenbacher, Tibor Gordon, Iouli E. Mikhailenko, Semen N. Shirin, Sergei V. TI IUPAC critical evaluation of the rotational-vibrational spectra of water vapor. Part I-Energy levels and transition wavenumbers for (H2O)-O-17 and (H2O)-O-18 SO JOURNAL OF QUANTITATIVE SPECTROSCOPY & RADIATIVE TRANSFER LA English DT Review DE Water vapor; Transition wavenumbers; Atmospheric physics; Energy levels; MARVEL; Information system; Database; Infrared spectra; Microwave spectra ID SUBMILLIMETER MICROWAVE-SPECTRUM; LORENTZ-BROADENING COEFFICIENTS; CENTRIFUGAL-DISTORTION ANALYSIS; FOURIER-TRANSFORM SPECTROSCOPY; RESOLUTION INFRARED SPECTRA; LINE-SHIFT COEFFICIENTS; RING-DOWN SPECTROSCOPY; 1.39 MU-M; INTERACTING STATES; ABSORPTION-SPECTRA AB This is the first part of a series of articles reporting critically evaluated rotational-vibrational line positions, transition intensities, pressure dependence and energy levels, with associated critically reviewed assignments and uncertainties, for all the main isotopologues of water. The present article contains energy levels and data for line positions of the singly substituted isotopologues (H2O)-O-17 and (H2O)-O-18. The procedure and code MARVEL, standing for measured active rotational-vibrational energy levels, is used extensively in all stages of determining the validated levels and lines and their self-consistent uncertainties. The spectral regions covered for both isotopologues (H2O)-O-17 and (H2O)-O-18 are 0-17 125 cm(-1). The energy levels are checked against ones determined from accurate variational calculations. The number of critically evaluated and recommended levels and lines are, respectively, 2687 and 8614 for (H2O)-O-17, and 4839 and 29364 for (H2O)-O-18. The extensive lists of MARVEL lines and levels obtained are deposited in the Supplementary Material, as well as in a distributed information system applied to water, W@DIS, where they can easily be retrieved. A distinguishing feature of the present evaluation of water spectroscopic data is the systematic use of all available experimental data and validation by first-principles theoretical calculations. (c) 2009 Elsevier Ltd. All rights reserved. C1 [Tennyson, Jonathan; Polyansky, Oleg L.] UCL, Dept Phys & Astron, London WC1E 6BT, England. [Bernath, Peter F.] Univ York, York YO10 5DD, N Yorkshire, England. [Brown, Linda R.; Toth, Robert A.] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Campargue, Alain] Univ Grenoble 1, Grenoble, France. [Carleere, Michel R.] Univ Libre Brussels, Brussels, Belgium. [Csaszar, Attila G.; Furtenbacher, Tibor] Eotvos Lorand Univ, Budapest, Hungary. [Gamache, Robert R.] Univ Massachusetts, Lowell, MA USA. [Hodges, Joseph T.] Natl Inst Stand & Technol, Gaithersburg, MD 20899 USA. [Jenouvrier, Alain; Daumont, Ludovic] Univ Reims, Reims, France. [Naumenko, Olga V.; Fazliev, Alexander Z.; Mikhailenko, Semen N.] Russian Acad Sci, Inst Atmospher Opt, Tomsk, Russia. [Rothman, Laurence S.; Gordon, Iouli E.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Vandaele, Ann Carine] Inst Aeron Spatiale Belgique, B-1180 Brussels, Belgium. [Zobov, Nikolai F.; Shirin, Sergei V.] Russian Acad Sci, Inst Appl Phys, Nizhnii Novgorod 603600, Russia. RP Tennyson, J (reprint author), UCL, Dept Phys & Astron, Mortimer St, London WC1E 6BT, England. EM j.tennyson@ucl.ac.uk RI Csaszar, Attila/A-5241-2009; Bernath, Peter/B-6567-2012; Hodges, Joseph/B-4578-2009; Tennyson, Jonathan/I-2222-2012; OI Rothman, Laurence/0000-0002-3837-4847; Bernath, Peter/0000-0002-1255-396X; Tennyson, Jonathan/0000-0002-4994-5238; Gordon, Iouli/0000-0003-4763-2841 FU Union of Pure and Applied Chemistry [2004-035-1-100]; UK Engineering and Physical Science Research Council; UK Natural Environment Research Council; Royal Society; British Council; INTAS foundation [WWLC-008535-MCA FP6 EC]; Scientific Research Fund of Hungary [OTKA T47185, K72885]; NKTH; European Union QUASAAR Marie Curie research training network; NATO; Russian Foundation for Basic Research; Belgian Federal Science Policy Office [EV/35/3A, SD/AT/01A, PRODEX 151490INLSFe(IC)]; Belgian National Fund for Scientific Research (FRFC contracts); Communaut de Belgique (Action de Recherche Concertees); NASA Earth Observing System (EOS) [NAG5-13534]; NASA laboratory astrophysics program; Programme National LEFE (CHAT) of CNRS (INSU); The National Aeronaudcs and Space Administratio FX We all thank the international Union of Pure and Applied Chemistry for funding under Project 2004-035-1-100 (A database of water transitions from experiment and theory). In addition, this work has received partial support from the UK Engineering and Physical Science Research Council, the UK Natural Environment Research Council, the Royal Society, the British Council, the INTAS foundation, Grant WWLC-008535-(reintegration) MCA FP6 EC, the Scientific Research Fund of Hungary (Grants OTKA T47185 and K72885), the NKTH, the European Union QUASAAR Marie Curie research training network, NATO, the Russian Foundation for Basic Research, the Belgian Federal Science Policy Office (Contracts EV/35/3A, SD/AT/01A, PRODEX 151490INLSFe(IC)), the Belgian National Fund for Scientific Research (FRFC contracts), the Communaut de Belgique (Action de Recherche Concertees), NASA Earth Observing System (EOS), under the Grant NAG5-13534, the NASA laboratory astrophysics program. Alain Campargue and Ludovic Daumont are grateful for the financial support provided by the Programme National LEFE (CHAT) of CNRS (INSU). Part of the research described in this paper was performed at the jet Propulsion Laboratory, California Institute of Technology, under contract with The National Aeronaudcs and Space Administration. NR 127 TC 90 Z9 95 U1 4 U2 28 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 JUN-JUL PY 2009 VL 110 IS 9-10 SI SI BP 573 EP 596 DI 10.1016/j.jqsrt.2009.02.014 PG 24 WC Optics; Spectroscopy SC Optics; Spectroscopy GA 447HD UT WOS:000266181300003 ER PT J AU Dick, MJ Drouin, BJ Pearson, JC AF Dick, Michael J. Drouin, Brian J. Pearson, John C. TI A collisional cooling investigation of the pressure broadening of the 1(10) <- 1(01) transition of water from 17 to 200 K SO JOURNAL OF QUANTITATIVE SPECTROSCOPY & RADIATIVE TRANSFER LA English DT Article DE Water; Pressure broadening; Collisional cooling; Temperature dependence ID VERY-LOW TEMPERATURE; EXCITATION RATES; ROTATIONAL-EXCITATION; INDUCED LINESHAPE; CARBON-MONOXIDE; VAPOR LINES; SHIFT; H2O; GHZ; H-2 AB An investigation of the 1(10)<- 1(01), rotational transition of water at 556 GHz pressure broadened by hydrogen, helium, nitrogen, oxygen and carbon dioxide has been completed. Using the collisional cooling technique the broadening of this transition by each gas was explored from 200 K down to the condensation point of the broadening gas or 17 K, which ever is lower. This marks the first time such an extensive investigation of the broadening of this rotational transition as a function of temperature has been completed. The results of this investigation will be presented including the exponential temperature dependence of the broadening, the lack of temperature dependence of the broadening observed in helium and the unique behavior of the hydrogen broadening at low temperature (< 40 K). In addition, the broadening of the 1(10)<- 1(01), rotational transition of water by nitrogen and oxygen was recorded at room temperature and a direct comparison of this data with recent work will be discussed. (c) 2008 Elsevier Ltd. All rights reserved. C1 [Dick, Michael J.; Drouin, Brian J.; Pearson, John C.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Dick, MJ (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM mdick@jpl.nasa.gov FU Jet Propulsion Laboratory, California Institute of Technology; National Aeronautics and Space Administration FX This work was performed at the Jet Propulsion Laboratory, California Institute of Technology under contract with the National Aeronautics and Space Administration. NR 26 TC 18 Z9 19 U1 0 U2 7 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 JUN-JUL PY 2009 VL 110 IS 9-10 SI SI BP 619 EP 627 DI 10.1016/j.jqsrt.2008.11.012 PG 9 WC Optics; Spectroscopy SC Optics; Spectroscopy GA 447HD UT WOS:000266181300006 ER PT J AU Dick, MJ Drouin, BJ Crawford, TJ Pearson, JC AF Dick, Michael J. Drouin, Brian J. Crawford, Timothy J. Pearson, John C. TI Pressure broadening of the J=5 <- 4 transition of carbon monoxide from 17 to 200 K: A new collisional cooling experiment SO JOURNAL OF QUANTITATIVE SPECTROSCOPY & RADIATIVE TRANSFER LA English DT Article DE Carbon monoxide; Pressure broadening; Collisional cooling; Collisional spectroscopy; Temperature dependence; Line shapes ID FUNDAMENTAL-BAND; ROTATIONAL TRANSITION; INDUCED LINESHAPE; LOW-TEMPERATURES; SPECTRAL-LINES; HALF-WIDTHS; WATER-VAPOR; CO; N-2; HELIUM AB A new spectroscopic experiment has been constructed at the jet Propulsion Laboratory. This experiment employs the collisional cooling technique to study gases at temperatures below their condensation points. Specifically, the experiment has been designed to mimic the temperatures of the interstellar medium for the study of water under these conditions. The ultimate purpose is to measure state-to-state excitation rates under equilibrium conditions to provide insights into the interpretation of interstellar water spectra obtained from space-borne platforms such as the Herschel Space Observatory. This paper presents an overview of the new experiment including a discussion of its design and a detailed explanation of the system. In addition, we report a pressure broadening study of the J = 5 <- 4 transition of CO at 576 GHz used as a system validation. The new results are compared with measurements from the literature as a validation of the new experiment. In addition, the non-classical behavior of the pressure broadening of CO at low temperature observed in the measurements will be discussed. (c) 2008 Elsevier Ltd. All rights reserved. C1 [Dick, Michael J.; Drouin, Brian J.; Crawford, Timothy J.; Pearson, John C.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Dick, MJ (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM mdick@jpl.nasa.gov RI Sung, Keeyoon/I-6533-2015 FU Jet Propulsion Laboratory, California Institute of Technology; National Aeronautics and Space Administration FX This work was performed at the Jet Propulsion Laboratory, California Institute of Technology under contract with the National Aeronautics and Space Administration. NR 29 TC 12 Z9 12 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 JUN-JUL PY 2009 VL 110 IS 9-10 BP 628 EP 638 DI 10.1016/j.jqsrt.2008.11.004 PG 11 WC Optics; Spectroscopy SC Optics; Spectroscopy GA 447HD UT WOS:000266181300007 ER PT J AU Smith, MAH Benner, DC Predoi-Cross, A Devi, VM AF Smith, M. A. H. Benner, D. Chris Predoi-Cross, A. Devi, V. Malathy TI Multispectrum analysis of (CH4)-C-12 in the nu(4) band: I. Air-broadened half widths, pressure-induced shifts, temperature dependences and line mixing SO JOURNAL OF QUANTITATIVE SPECTROSCOPY & RADIATIVE TRANSFER LA English DT Article DE Methane; Air broadening; Pressure-induced shifts; Temperature dependence; Off-diagonal relaxation matrix elements; Line mixing; FTIR spectroscopy ID TUNABLE DIODE-LASER; METHANE LINES; SPECTRAL REGION; NU(3) BAND; Q-BRANCH; ATMOSPHERIC METHANE; COEFFICIENTS WIDTHS; CM(-1) REGION; 2-NU(3) BAND; 2V(3) BAND AB Lorentz air-broadened half widths, pressure-induced shifts and their temperature dependences have been measured for over 430 transitions (allowed and forbidden) in the nu(4) band of (CH4)-C-12 over the temperature range 210-314 K. A multispectrum non linear least squares fitting technique was used to simultaneously fit a large number of high-resolution (0.006-0.01 cm(-1)) absorption spectra of pure methane and mixtures of methane diluted with dry air. Line mixing was detected for pairs of A-, E-, and F-species transitions in the P- and R-branch manifolds and quantified using the off-diagonal relaxation matrix elements formalism. The measured parameters are compared to air- and N-2-broadened values reported in the literature for the nu(4) and other bands. The dependence of the various spectral line parameters upon the tetrahedral symmetry species and rotational quantum numbers of the transitions is discussed. All data used in the present work were recorded using the McMath-Pierce Fourier transform spectrometer located at the National Solar Observatory on Kitt Peak. Published by Elsevier Ltd. C1 [Smith, M. A. H.] NASA, Langley Res Ctr, Sci Directorate, Hampton, VA 23681 USA. [Benner, D. Chris; Devi, V. Malathy] Coll William & Mary, Williamsburg, VA 23187 USA. [Predoi-Cross, A.] Univ Lethbridge, Dept Phys, Lethbridge, AB T1K 3M4, Canada. RP Smith, MAH (reprint author), NASA, Langley Res Ctr, Sci Directorate, Hampton, VA 23681 USA. EM Mary.Ann.H.Smith@nasa.gov FU National Aeronautics and Space Administration; National Sciences and Engineering Research Council of Canada (NSERC); NASA's Upper Atmosphere Research Program FX The authors thank Claude Plymate and Mike Dulick of the NSO for their assistance with the FTS laboratory measurements at Kitt Peak. We also thank Linda Brown of the jet Propulsion Laboratory for reading the manuscript and providing helpful comments. Research at the College of William and Mary is supported under contracts and cooperative agreements with the National Aeronautics and Space Administration. A. Predoi-Cross acknowledges the support received from the National Sciences and Engineering Research Council of Canada (NSERC). NASA's Upper Atmosphere Research Program provides funding to the NSO for support of NASA activities at the McMath-Pierce FTS laboratory facility. NR 57 TC 17 Z9 18 U1 2 U2 13 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 JUN-JUL PY 2009 VL 110 IS 9-10 SI SI BP 639 EP 653 DI 10.1016/j.jqsrt.2009.02.015 PG 15 WC Optics; Spectroscopy SC Optics; Spectroscopy GA 447HD UT WOS:000266181300008 ER PT J AU Asnani, V Delap, D Creager, C AF Asnani, Vivake Delap, Damon Creager, Colin TI The development of wheels for the Lunar Roving Vehicle SO JOURNAL OF TERRAMECHANICS LA English DT Article CT Annual Meeting of the Japanese-Society-for-Terramechanics CY JUN 23-26, 2007 CL Fairbanks, AK SP Japanese Soc Terrmechan AB The Lunar Roving Vehicle (LRV) was developed for NASA's Apollo program so astronauts could cover a greater range oil the lunar surface, carry more science instruments, and return more soil and rock samples than by foot. Because of the unique lunar environment, the creation of flexible wheels was the most challenging and time consuming aspect of the LRV development. Wheels developed for previous lunar systems were not sufficient for use with this manned vehicle; therefore, several new designs were created and tested. Based oil criteria set by NASA, the choices were narrowed down to two: the wire mesh wheel developed by General Motors, and the hoop spring wheel developed by the Bendix Corporation. Each of these underwent intensive mechanical, material, and terramechanical analyses, and in the end, the wire mesh wheel was chosen for the LRV. Though the wire mesh wheel was determined to be the best choice for its particular application, it may be insufficient towards achieving the objectives of future lunar missions that could require higher tractive capability, increased weight capacity, or extended life. Therefore lessons learned from the original LRV wheel development and suggestions for future Moon wheel projects are offered. Published by Elsevier Ltd. C1 [Asnani, Vivake; Delap, Damon; Creager, Colin] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. RP Asnani, V (reprint author), NASA, Glenn Res Ctr, 21000 Brookpk Rd,MS 23-3, Cleveland, OH 44135 USA. EM vivake.m.asnani@nasa.gov NR 31 TC 16 Z9 23 U1 0 U2 7 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0022-4898 J9 J TERRAMECHANICS JI J. Terramech. PD JUN PY 2009 VL 46 IS 3 BP 89 EP 103 DI 10.1016/j.jterra.2009.02.005 PG 15 WC Engineering, Environmental SC Engineering GA 458DI UT WOS:000266993900004 ER PT J AU Hoff, RM Christopher, SA AF Hoff, Raymond M. Christopher, Sundar A. TI Remote Sensing of Particulate Pollution from Space: Have We Reached the Promised Land? SO JOURNAL OF THE AIR & WASTE MANAGEMENT ASSOCIATION LA English DT Review ID AEROSOL OPTICAL-THICKNESS; GROUND-LEVEL PM2.5; MATTER AIR-QUALITY; FIRE RADIATIVE ENERGY; SATELLITE DATA; UNITED-STATES; LIGHT-SCATTERING; STRATOSPHERIC AEROSOL; RADIANCE MEASUREMENTS; ATMOSPHERIC AEROSOLS AB The recent literature on satellite remote sensing of air quality is reviewed. 2009 is the 50th anniversary of the first satellite atmospheric observations. For the first 40 of those years, atmospheric composition measurements, meteorology, and atmospheric structure and dynamics dominated the missions launched. Since 1995, 42 instruments relevant to air quality measurements have been put into orbit. Trace gases such as ozone, nitric oxide, nitrogen dioxide, water, oxygen/tetraoxygen, bromine oxide, sulfur dioxide, formaldehyde, glyoxal, chlorine dioxide, chlorine monoxide, and nitrate radical have been measured in the stratosphere and troposphere in column measurements. Aerosol optical depth (AOD) is a focus of this review and a significant body of literature exists that shows that ground-level fine particulate matter (PM2.5) can be estimated from columnar AOD. Precision of the measurement of AOD is +/-20% and the prediction of PM,., from AOD is order +/-30% in the most careful studies. The air quality needs that can use such predictions are examined. Satellite measurements are important to event detection, transport and model prediction, and emission estimation. It is suggested that ground-based measurements, models, and satellite measurements should be viewed as a system, each component of which is necessary to better understand air quality. C1 [Hoff, Raymond M.] Univ Maryland, Goddard Earth Sci & Technol Ctr, Joint Ctr Earth Syst Technol, Baltimore, MD 21250 USA. [Hoff, Raymond M.] Univ Maryland, Dept Phys, Baltimore, MD 21250 USA. [Christopher, Sundar A.] Univ Alabama, Dept Atmospher Sci, Huntsville, AL 35899 USA. [Christopher, Sundar A.] Univ Alabama, Ctr Earth Syst Sci, Huntsville, AL 35899 USA. RP Hoff, RM (reprint author), Univ Maryland, Goddard Earth Sci & Technol Ctr, Joint Ctr Earth Syst Technol, 1000 Hilltop Circle, Baltimore, MD 21250 USA. EM hoff@umbc.edu RI Christopher, Sundar/E-6781-2011; Hoff, Raymond/C-6747-2012 NR 224 TC 173 Z9 178 U1 18 U2 86 PU TAYLOR & FRANCIS INC PI PHILADELPHIA PA 530 WALNUT STREET, STE 850, PHILADELPHIA, PA 19106 USA SN 1096-2247 EI 2162-2906 J9 J AIR WASTE MANAGE JI J. Air Waste Manage. Assoc. PD JUN PY 2009 VL 59 IS 6 BP 645 EP 675 DI 10.3155/1047-3289.59.6.645 PG 31 WC Engineering, Environmental; Environmental Sciences; Meteorology & Atmospheric Sciences SC Engineering; Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences GA 455WB UT WOS:000266797400002 PM 19603734 ER PT J AU Generazio, ER AF Generazio, E. R. TI Design of Experiments for Validating Probability of Detection Capability of NDT Systems and for Qualification of Inspectors SO MATERIALS EVALUATION LA English DT Article DE probability of detection; design of experiments; fracture critical; nondestructive testing; quality assurance AB The capability of a testing system is established by application of various methodologies to determine the probability of detection (POD). One accepted metric of an adequate testing system is that there is 95% confidence that the POD is greater than 90% (90/95 POD). Design of experiments for validating probability of detection (DOEPOD) capability of nondestructive testing systems is a diagnostic tool providing detailed analysis of POD test data, guidance on establishing data distribution requirements and resolving test issues. DOEPOD demands utilization of observation of occurrences. The DOEPOD capability has been developed to provide an efficient and accurate methodology that yields observed POD and confidence limits for both hit/miss or signal amplitude testing. DOEPOD does not assume prescribed POD logarithmic or similar functions with assumed adequacy over a wide range of discontinuity sizes and testing system technologies, so multiparameter curve fitting or model optimization approaches to generate a POD curve are not required. DOEPOD applications for supporting inspector qualifications are discussed. C1 NASA, Langley Res Ctr, Hampton, VA 23681 USA. RP Generazio, ER (reprint author), NASA, Langley Res Ctr, MS 231,Bldg 1230B,Room 189, Hampton, VA 23681 USA. EM edward.r.generazio@nasa.gov NR 10 TC 5 Z9 5 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 JUN PY 2009 VL 67 IS 6 BP 730 EP 738 PG 9 WC Materials Science, Characterization & Testing SC Materials Science GA 459QK UT WOS:000267118400016 ER PT J AU Bogard, D Park, J Garrison, D AF Bogard, Donald Park, Jisun Garrison, Daniel TI Ar-39-Ar-40 "ages" and origin of excess Ar-40 in Martian shergottites SO METEORITICS & PLANETARY SCIENCE LA English DT Article ID AL GANI 476/489; NOBLE-GASES; SNC METEORITES; DIFFERENTIATION HISTORY; BASALTIC SHERGOTTITES; ISOTOPIC SYSTEMATICS; ZAGAMI METEORITE; EJECTION TIMES; LOS-ANGELES; PARENT BODY AB We report new Ar-39-Ar-40 Measurements oil 15 plagioclase, pyroxene, and/or whole rock samples of 8 Martian shergottites. All age spectra suggest ages older than the meteorite formation ages, as defined by Sm-Nd and Rb-Sr isochrons. Employing isochron plots, only Los Angeles plagioclase and possibly Northwest Africa (NWA) 3 17 1 plagioclase give ages in agreement with their formation ages. Isochrons for all shergottite samples reveal the presence of trapped Martian Ar-40 (Ar-40(xs)), which exists in variable amounts ill different lattice locations. Some Ar-40(xs) is uniformly distributed throughout the lattice, resulting ill a positive isochron intercept, and Other Ar-40(xs) Occurs ill association with K-bearing minerals and increases the isochron slope. These samples demonstrate Situations where linear Ar isochrons give false ages that are too old. After Subtracting Ar-40-* that would accumulate by K-40 decay since meteorite formation and small amounts of terrestrial Ar-40, all Young age samples give similar Ar-40(xs) concentrations of similar to 1-2 x 10(-6) cm(3)/g, but a variation in K content by a factor of similar to 80. Previously reported NASA Johnson Space Center data for Zagami, Shergotty, Yamato (Y-) 000097, Y-793605, and Queen Alexandra Range (QUE) 94201 shergottites show similar concentrations of Ar-40(xs) to the new meteorite data reported here. Similar Ar-40(xs) in different minerals and meteorites cannot be explained as arising from Martian atmosphere carried ill strongly shocked phases Such as melt veins. We invoke the explanation given by Bogard and Park (2008) for Zagami, that this Ar-40(xs) in shergottites, was acquired from the magma. Similarity in Ar-40(xs) among shergottites may reveal common magma Sources and/or similar magma generation and emplacement processes. C1 [Bogard, Donald; Park, Jisun; Garrison, Daniel] NASA, Lyndon B Johnson Space Ctr, ARES, Code KR, Houston, TX 77058 USA. [Garrison, Daniel] ESCG Barrios, Houston, TX 77058 USA. RP Bogard, D (reprint author), NASA, Lyndon B Johnson Space Ctr, ARES, Code KR, Houston, TX 77058 USA. EM donald.d.bogard@nasa.gov FU NASA FX This research was supported by NASA's Cosmochemistry Program. J. P. also acknowledges support of the NASA Postdoctoral Program. NR 85 TC 11 Z9 11 U1 3 U2 8 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 1086-9379 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD JUN PY 2009 VL 44 IS 6 BP 905 EP 923 PG 19 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 487OM UT WOS:000269284100009 ER PT J AU Coppin, KEK Smail, I Alexander, DM Weiss, A Walter, F Swinbank, AM Greve, TR Kovacs, A De Breuck, C Dickinson, M Ibar, E Ivison, RJ Reddy, N Spinrad, H Stern, D Brandt, WN Chapman, SC Dannerbauer, H van Dokkum, P Dunlop, JS Frayer, D Gawiser, E Geach, JE Huynh, M Knudsen, KK Koekemoer, AM Lehmer, BD Menten, KM Papovich, C Rix, HW Schinnerer, E Wardlow, JL van der Werf, PP AF Coppin, K. E. K. Smail, Ian Alexander, D. M. Weiss, A. Walter, F. Swinbank, A. M. Greve, T. R. Kovacs, A. De Breuck, C. Dickinson, M. Ibar, E. Ivison, R. J. Reddy, N. Spinrad, H. Stern, D. Brandt, W. N. Chapman, S. C. Dannerbauer, H. van Dokkum, P. Dunlop, J. S. Frayer, D. Gawiser, E. Geach, J. E. Huynh, M. Knudsen, K. K. Koekemoer, A. M. Lehmer, B. D. Menten, K. M. Papovich, C. Rix, H. -W. Schinnerer, E. Wardlow, J. L. van der Werf, P. P. TI A submillimetre galaxy at z=4.76 in the LABOCA survey of the Extended Chandra Deep Field-South SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Review DE galaxies: evolution; galaxies: formation; galaxies: high-redshift; galaxies: individual: GDS J033229.29-275619.5; galaxies: individual: LESS J033229.4-275619; submillimetre ID DEGREE EXTRAGALACTIC SURVEY; DIGITAL SKY SURVEY; POINT-SOURCE CATALOGS; HIGH-REDSHIFT QUASARS; STELLAR POPULATIONS; RADIO GALAXIES; GOODS 850-5; VLT/FORS2 SPECTROSCOPY; PHOTOMETRIC REDSHIFTS; ENERGY-DISTRIBUTIONS AB We report on the identification of the highest redshift submillimetre-selected source currently known LESS J033229.4-275619. This source was detected in the Large Apex Bolometer Camera (LABOCA) Extended Chandra Deep Field-South (ECDF-S) Submillimetre Survey (LESS), a sensitive 870-mu m survey (sigma(870 mu m) similar to 1.2 mJy) of the full 30 x 30 arcmin(2) ECDF-S with the LABOCA on the Atacama Pathfinder Experiment telescope. The submillimetre emission is identified with a radio counterpart for which optical spectroscopy provides a redshift of z = 4.76. We show that the bolometric emission is dominated by a starburst with a star formation rate of similar to 1000 M(circle dot) yr(-1), although we also identify a moderate luminosity active galactic nucleus (AGN) in this galaxy. Thus it has characteristics similar to those of z similar to 2 submillimetre galaxies (SMGs), with a mix of starburst and obscured AGN signatures. This demonstrates that ultraluminous starburst activity is not just restricted to the hosts of the most luminous (and hence rare) quasi-stellar objects at z similar to 5, but was also occurring in less extreme galaxies at a time when the Universe was less than 10 per cent of its current age. Assuming that we are seeing the major phase of star formation in this galaxy, then we demonstrate that it would be identified as a luminous distant red galaxy at z similar to 3 and that the current estimate of the space density of z > 4 SMGs is only sufficient to produce greater than or similar to 10 per cent of the luminous red galaxy population at these early times. However, this leaves open the possibility that some of these galaxies formed through less intense, but more extended star formation events. If the progenitors of all of the luminous red galaxies at z similar to 3 go through an ultraluminous starburst at z greater than or similar to 4 then the required volume density of z > 4 SMGs will exceed that predicted by current galaxy formation models by more than an order of magnitude. C1 [Coppin, K. E. K.; Smail, Ian; Swinbank, A. M.; Geach, J. E.] Univ Durham, Inst Computat Cosmol, Durham DH1 3LE, England. [Alexander, D. M.; Lehmer, B. D.; Wardlow, J. L.] Univ Durham, Dept Phys, Durham DH1 3LE, England. [Weiss, A.; Kovacs, A.; Menten, K. M.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Walter, F.; Greve, T. R.; Dannerbauer, H.; Rix, H. -W.; Schinnerer, E.] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [De Breuck, C.] European So Observ, D-85748 Garching, Germany. [Dickinson, M.; Reddy, N.] Natl Opt Astron Observ, Tucson, AZ 85726 USA. [Ibar, E.; Ivison, R. J.; Dunlop, J. S.] Univ Edinburgh, Royal Observ, Inst Astron, SUPA, Edinburgh EH9 3HJ, Midlothian, Scotland. [Ivison, R. J.] Royal Observ, UK Astron Technol Ctr, Edinburgh EH9 3HJ, Midlothian, Scotland. [Spinrad, H.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Stern, D.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Brandt, W. N.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Chapman, S. C.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. [van Dokkum, P.] Yale Univ, Dept Astron, New Haven, CT 06520 USA. [Frayer, D.; Huynh, M.] CALTECH, Ctr Infrared Proc & Anal, Pasadena, CA 91125 USA. [Gawiser, E.] Rutgers State Univ, Dept Phys & Astron, Piscataway, NJ 08854 USA. [Knudsen, K. K.] Univ Bonn, Argelander Inst Astron, D-53121 Bonn, Germany. [Koekemoer, A. M.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Papovich, C.] Texas A&M Univ, Dept Phys, GP & CM Mitchell Inst Fundamental Phys, College Stn, TX 77843 USA. [van der Werf, P. P.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. RP Coppin, KEK (reprint author), Univ Durham, Inst Computat Cosmol, South Rd, Durham DH1 3LE, England. EM kristen.coppin@durham.ac.uk RI Smail, Ian/M-5161-2013; Wardlow, Julie/C-9903-2015; Brandt, William/N-2844-2015; Kovacs, Attila/C-1171-2010; Ivison, R./G-4450-2011; OI Smail, Ian/0000-0003-3037-257X; Wardlow, Julie/0000-0003-2376-8971; /0000-0002-0729-2988; Koekemoer, Anton/0000-0002-6610-2048; Brandt, William/0000-0002-0167-2453; Kovacs, Attila/0000-0001-8991-9088; Ivison, R./0000-0001-5118-1313; Knudsen, Kirsten Kraiberg/0000-0002-7821-8873; De Breuck, Carlos/0000-0002-6637-3315; Alexander, David/0000-0002-5896-6313; Schinnerer, Eva/0000-0002-3933-7677 FU Science and Technology Facilities Council (STFC); Royal Society; Lockyer; Chandra X-ray Observatory's [SP8-9003A]; W. M. Keck Foundation; NASA FX Observations have been carried out using APEX and the VLT under Program IDs: 080.A-3023, 079.F-9500, 170.A-0788, 074.A-0709 and 275.A-5060. APEX is operated by the Max-Planck-Institut fur Radioastronomie, the European Southern Observatory and the Onsala Space Observatory. We would like to thank the staff for their aid in carrying out the observations. Some of the data presented herein were obtained at the W. M. Keck Observatory, which is operated as a scientific partnership among Caltech, the University of California and NASA. The Keck Observatory was made possible by the generous financial support of the W. M. Keck Foundation. This work is based in part on observations from the Legacy Science Program, made with the Spitzer Space Telescope, which is operated by JPL, Caltech, under a contract with NASA; and support for this work was provided by NASA through an award issued by JPL/Caltech. This research has also made use of the NASA/IPAC Extragalactic Database (NED) which is operated by JPL/Caltech, under contract with NASA. Ned Wright's Javascript Cosmology Calculator was also used in preparing this paper (Wright 2006). NR 101 TC 94 Z9 94 U1 0 U2 3 PU WILEY-BLACKWELL PUBLISHING, INC PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD JUN 1 PY 2009 VL 395 IS 4 BP 1905 EP 1914 DI 10.1111/j.1365-2966.2009.14700.x PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 446HL UT WOS:000266112600009 ER PT J AU Croston, JH Kraft, RP Hardcastle, MJ Birkinshaw, M Worrall, DM Nulsen, PEJ Penna, RF Sivakoff, GR Jordan, A Brassington, NJ Evans, DA Forman, WR Gilfanov, M Goodger, JL Harris, WE Jones, C Juett, AM Murray, SS Raychaudhury, S Sarazin, CL Voss, R Woodley, KA AF Croston, J. H. Kraft, R. P. Hardcastle, M. J. Birkinshaw, M. Worrall, D. M. Nulsen, P. E. J. Penna, R. F. Sivakoff, G. R. Jordan, A. Brassington, N. J. Evans, D. A. Forman, W. R. Gilfanov, M. Goodger, J. L. Harris, W. E. Jones, C. Juett, A. M. Murray, S. S. Raychaudhury, S. Sarazin, C. L. Voss, R. Woodley, K. A. TI High-energy particle acceleration at the radio-lobe shock of Centaurus A SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE shock waves; galaxies: active; galaxies: elliptical and lenticular: cD; galaxies: individual: Cen A; radio continuum: galaxies; X-rays: galaxies ID MAGNETIC-FIELD STRENGTHS; DEEP CHANDRA OBSERVATION; COSMIC-RAY ACCELERATION; X-RAY; SUPERNOVA-REMNANTS; PERSEUS CLUSTER; HOT GAS; GALAXY; EMISSION; NUCLEUS AB We present new results on the shock around the south-west radio lobe of Centaurus A using data from the Chandra Very Large Programme observations (740 ks total observing time). The X-ray spectrum of the emission around the outer south-western edge of the lobe is well described by a single power-law model with Galactic absorption - thermal models are strongly disfavoured, except in the region closest to the nucleus. We conclude that a significant fraction of the X-ray emission around the south-west part of the lobe is synchrotron, not thermal. We infer that in the region where the shock is strongest and the ambient gas density lowest, the inflation of the lobe is accelerating particles to X-ray synchrotron emitting energies, similar to supernova remnants such as SN1006. This interpretation resolves a problem of our earlier, purely thermal, interpretation for this emission, namely that the density compression across the shock was required to be much larger than the theoretically expected factor of 4. We describe a self-consistent model for the lobe dynamics and shock properties using the shell of thermal emission to the north of the lobe to estimate the lobe pressure. Based on this model, we estimate that the lobe is expanding to the south-west with a velocity of similar to 2600 km s(-1), roughly Mach 8 relative to the ambient medium. We discuss the spatial variation of spectral index across the shock region, concluding that our observations constrain gamma(max) for the accelerated particles to be similar to 10(8) at the strongest part of the shock, consistent with expectations from diffusive shock acceleration theory. Finally, we consider the implications of these results for the production of ultra-high energy cosmic rays (UHECRs) and TeV emission from Centaurus A, concluding that the shock front region is unlikely to be a significant source of UHECRs, but that TeV emission from this region is expected at levels comparable to current limits at TeV energies, for plausible assumed magnetic field strengths. C1 [Croston, J. H.; Hardcastle, M. J.; Goodger, J. L.] Univ Hertfordshire, Sch Phys Astron & Math, Hatfield AL10 9AB, Herts, England. [Kraft, R. P.; Birkinshaw, M.; Worrall, D. M.; Nulsen, P. E. J.; Penna, R. F.; Jordan, A.; Brassington, N. J.; Evans, D. A.; Forman, W. R.; Jones, C.; Murray, S. S.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Sivakoff, G. R.; Sarazin, C. L.] Univ Virginia, Dept Astron, Charlottesville, VA 22904 USA. [Sivakoff, G. R.] Ohio State Univ, Dept Astron, McPherson Lab 4055, Columbus, OH 43210 USA. [Jordan, A.] Pontificia Univ Catolica Chile, Dept Astron & Astrofis, Santiago 22, Chile. [Evans, D. A.] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. [Gilfanov, M.; Voss, R.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Gilfanov, M.] Russian Acad Sci, Space Res Inst, Moscow 117997, Russia. [Harris, W. E.; Woodley, K. A.] McMaster Univ, Dept Phys & Astron, Hamilton, ON L8S 4M1, Canada. [Juett, A. M.] NASA, Goddard Space Flight Ctr, Lab Xray Astrophys, Greenbelt, MD 20771 USA. [Voss, R.] Tech Univ Munich, Excellence Cluster Universe, D-85748 Garching, Germany. [Raychaudhury, S.] Univ Birmingham, Sch Phys & Astron, Birmingham B15 2TT, W Midlands, England. [Birkinshaw, M.; Worrall, D. M.] Univ Bristol, HH Wills Phys Lab, Bristol BS8 1TL, Avon, England. RP Croston, JH (reprint author), Univ Hertfordshire, Sch Phys Astron & Math, Coll Lane, Hatfield AL10 9AB, Herts, England. EM J.H.Croston@herts.ac.uk RI Hardcastle, Martin/E-2264-2012; Sivakoff, Gregory/G-9602-2011; OI Hardcastle, Martin/0000-0003-4223-1117; Sivakoff, Gregory/0000-0001-6682-916X; Nulsen, Paul/0000-0003-0297-4493; Goodger, Joanna/0000-0002-5738-4768; Jordan, Andres/0000-0002-5389-3944 FU NASA [NAS8-03060, GO7-8105X]; Hubble [HST-GO-10597.03-A]; Royal Society FX This work was partially supported by NASA grants NAS8-03060 and GO7-8105X, and Hubble grant HST-GO-10597.03-A. We gratefully acknowledge support from the Royal Society (research fellowship for MJH). NR 52 TC 63 Z9 63 U1 0 U2 3 PU WILEY-BLACKWELL PUBLISHING, INC PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD JUN 1 PY 2009 VL 395 IS 4 BP 1999 EP 2012 DI 10.1111/j.1365-2966.2009.14715.x PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 446HL UT WOS:000266112600018 ER PT J AU Steffen, CJ Freeh, JE Linne, DL Faykus, EW Gallo, CA Green, RD AF Steffen, Christopher J., Jr. Freeh, Joshua E. Linne, Diane L. Faykus, Eric W. Gallo, Christopher A. Green, Robert D. TI SYSTEM MODELING OF LUNAR OXYGEN PRODUCTION USING FISSION SURFACE POWER: MASS AND POWER REQUIREMENTS SO NUCLEAR TECHNOLOGY LA English DT Article; Proceedings Paper CT Space Nuclear Conference (SNC 07) held at the Annual Meeting of the American-Nuclear-Society CY JUN 24-28, 2007 CL Boston, MA SP Amer Nucl Soc DE in situ resource utilization; oxygen production; water splitting AB A method for estimating the mass and fission surface power requirements of a lunar oxygen production facility is introduced. The individual modeling components involve the chemical processing and cryogenic storage subsystems needed to process a beneficiated regolith stream into liquid oxygen via ilmenite reduction. The power can be supplied from one of six different fission reactor-converter systems. A baseline system analysis, capable of producing 15 tonnes/yr of oxygen, is presented. The influence of reactor-converter choice was seen to have a small but measurable impact on the system configuration and performance. Finally, the mission concept of operations can have a substantial impact upon individual component size and power requirements. C1 [Steffen, Christopher J., Jr.; Freeh, Joshua E.; Linne, Diane L.; Faykus, Eric W.; Gallo, Christopher A.; Green, Robert D.] NASA Glenn Res Ctr, Cleveland, OH 44135 USA. RP Steffen, CJ (reprint author), NASA Glenn Res Ctr, Cleveland, OH 44135 USA. EM Christopher.J.Steffen@NASA.gov NR 22 TC 1 Z9 1 U1 0 U2 3 PU AMER NUCLEAR SOC PI LA GRANGE PK PA 555 N KENSINGTON AVE, LA GRANGE PK, IL 60526 USA SN 0029-5450 J9 NUCL TECHNOL JI Nucl. Technol. PD JUN PY 2009 VL 166 IS 3 BP 240 EP 251 PG 12 WC Nuclear Science & Technology SC Nuclear Science & Technology GA 447WC UT WOS:000266221700005 ER PT J AU Schwarz, C Debruyne, R Kuch, M McNally, E Schwarcz, H Aubrey, AD Bada, J Poinar, H AF Schwarz, Carsten Debruyne, Regis Kuch, Melanie McNally, Elizabeth Schwarcz, Henry Aubrey, Andrew D. Bada, Jeffrey Poinar, Hendrik TI New insights from old bones: DNA preservation and degradation in permafrost preserved mammoth remains SO NUCLEIC ACIDS RESEARCH LA English DT Article ID ANCIENT HUMAN DNA; DEOXYRIBONUCLEIC-ACID; NEANDERTHAL DNA; SEQUENCES; DAMAGE; RETRIEVAL; CRYSTALLINITY; AMPLIFICATION; MITOCHONDRIA; ENANTIOMERS AB Despite being plagued by heavily degraded DNA in palaeontological remains, most studies addressing the state of DNA degradation have been limited to types of damage which do not pose a hindrance to Taq polymerase during PCR. Application of serial qPCR to the two fractions obtained during extraction (demineralization and protein digest) from six permafrost mammoth bones and one partially degraded modern elephant bone has enabled further insight into the changes which endogenous DNA is subjected to during diagenesis. We show here that both fractions exhibit individual qualities in terms of the prevailing type of DNA (i.e. mitochondrial versus nuclear DNA) as well as the extent of damage, and in addition observed a highly variable ratio of mitochondrial to nuclear DNA among the six mammoth samples. While there is evidence suggesting that mitochondrial DNA is better preserved than nuclear DNA in ancient permafrost samples, we find the initial DNA concentration in the bone tissue to be as relevant for the total accessible mitochondrial DNA as the extent of DNA degradation post-mortem. We also evaluate the general applicability of indirect measures of preservation such as amino-acid racemization, bone crystallinity index and thermal age to these exceptionally well-preserved samples. C1 [Schwarz, Carsten; Debruyne, Regis; Kuch, Melanie; Poinar, Hendrik] McMaster Univ, McMaster Ancient DNA Ctr, Dept Anthropol, Hamilton, ON, Canada. [McNally, Elizabeth] McMaster Univ, Dept Mat Sci & Engn, Hamilton, ON, Canada. [Schwarcz, Henry] McMaster Univ, Sch Geog & Earth Sci, Hamilton, ON, Canada. [Aubrey, Andrew D.] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Bada, Jeffrey] Univ Calif San Diego, Scripps Inst Oceanog, La Jolla, CA 92093 USA. [Poinar, Hendrik] McMaster Univ, Michael DeGroote Inst Infect Dis Res, Hamilton, ON, Canada. RP Poinar, H (reprint author), McMaster Univ, McMaster Ancient DNA Ctr, Dept Anthropol, 1280 Main St W, Hamilton, ON, Canada. EM poinarh@mcmaster.ca RI Debruyne, Regis/G-7839-2011 FU Natural Science and Engineering Research Council [299103-2004]; Social Sciences and Humanities Research Council [410-2004-0579]; Canadian Research Chairs Program; McMaster University FX Natural Science and Engineering Research Council ( grant #299103-2004); Social Sciences and Humanities Research Council grant (#410-2004-0579); the Canadian Research Chairs Program and McMaster University. Funding for open access charge: Natural Sciences and Engineering Research Council of Canada (NSERC). NR 41 TC 65 Z9 66 U1 4 U2 25 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0305-1048 J9 NUCLEIC ACIDS RES JI Nucleic Acids Res. PD JUN PY 2009 VL 37 IS 10 BP 3215 EP 3229 DI 10.1093/nar/gkp159 PG 15 WC Biochemistry & Molecular Biology SC Biochemistry & Molecular Biology GA 457WU UT WOS:000266966700009 PM 19321502 ER PT J AU Lindstrom, EJ Kendall, JJ Chicoski, B AF Lindstrom, Eric J. Kendall, James J., Jr. Chicoski, Benjamin TI TEN YEARS OF NOPP ACCOMPLISHMENTS SO OCEANOGRAPHY LA English DT Editorial Material C1 [Lindstrom, Eric J.] Natl Aeronaut & Space Adm, Div Earth Sci, Washington, DC USA. [Kendall, James J., Jr.] Minerals Management Serv, Herndon, VA USA. [Chicoski, Benjamin] Consortium Ocean Leadership, Fed Interagcy Programs, Washington, DC USA. RP Lindstrom, EJ (reprint author), Natl Aeronaut & Space Adm, Div Earth Sci, Washington, DC USA. EM eric.j.lindstrom@nasa.gov NR 0 TC 0 Z9 0 U1 0 U2 0 PU OCEANOGRAPHY SOC PI ROCKVILLE PA P.O. BOX 1931, ROCKVILLE, MD USA SN 1042-8275 J9 OCEANOGRAPHY JI Oceanography PD JUN PY 2009 VL 22 IS 2 BP 25 EP 27 PG 3 WC Oceanography SC Oceanography GA 457WC UT WOS:000266964200008 ER PT J AU Chassignet, EP Hurlburt, HE Metzger, EJ Smedstad, OM Cummings, JA Halliwell, GR Bleck, R Baraille, R Wallcraft, AJ Lozano, C Tolman, HL Srinivasan, A Hankin, S Cornillon, P Weisberg, R Barth, A He, R Werner, F Wilkin, J AF Chassignet, Eric P. Hurlburt, Harley E. Metzger, E. Joseph Smedstad, Ole Martin Cummings, James A. Halliwell, George R. Bleck, Rainer Baraille, Remy Wallcraft, Alan J. Lozano, Carlos Tolman, Hendrik L. Srinivasan, Ashwanth Hankin, Steve Cornillon, Peter Weisberg, Robert Barth, Alexander He, Ruoying Werner, Francisco Wilkin, John TI US GODAE Global Ocean Prediction with the HYbrid Coordinate Ocean Model (HYCOM) SO OCEANOGRAPHY LA English DT Article ID NORTH-ATLANTIC; VERTICAL COORDINATE; DATA ASSIMILATION; SYSTEM; 1/10-DEGREES; SIMULATION; SURFACE; IMPACT AB During the past five to ten years, a broad partnership of institutions under NOPP sponsorship has collaborated in developing and demonstrating the performance and application of eddy-resolving, real-time global- and basin-scale ocean prediction systems using the HYbrid Coordinate Ocean Model (HYCOM). The partnership represents a broad spectrum of the oceanographic community, bringing together academia, federal agencies, and industry/commercial entities, and spanning modeling, data assimilation, data management and serving, observational capabilities, and application of HYCOM prediction system outputs. In addition to providing real-time, eddy-resolving global- and basin-scale ocean prediction systems for the US Navy and NOAA, this project also offered an outstanding opportunity for NOAA-Navy collaboration and cooperation, ranging from research to the operational level. This paper provides an overview of the global HYCOM ocean prediction system and highlights some of its achievements. An important outcome of this effort is the capability of the global system to provide boundary conditions to even higher-resolution regional and coastal models. C1 [Chassignet, Eric P.] Florida State Univ, Ctr Ocean Atmospher Predict Studies, Tallahassee, FL 32306 USA. [Smedstad, Ole Martin] QinetiQ N Amer Technol Solut Grp, Stennis Space Ctr, MS USA. [Metzger, E. Joseph; Cummings, James A.; Wallcraft, Alan J.] USN, Res Lab, Ocean Dynam & Predict Branch, Stennis Space Ctr, MS USA. [Halliwell, George R.] NOAA, Atlantic Oceanog & Meteorol Lab, Miami, FL 33149 USA. [Bleck, Rainer] NASA, Goddard Inst Space Studies, New York, NY 10025 USA. [Bleck, Rainer] NOAA, Earth Syst Res Lab, Boulder, CO USA. [Baraille, Remy] Serv Hydrog & Oceanog Marine, Toulouse, France. [Tolman, Hendrik L.] NOAA, Natl Ctr Environm Predict, Environm Modeling Ctr, Marine Modeling & Anal Branch, Camp Springs, MD USA. [Srinivasan, Ashwanth] Univ Miami, Rosenstiel Sch Marine & Atmospher Sci, Div Meteorol & Oceanog, Miami, FL 33149 USA. [Hankin, Steve] NOAA, Pacific Marine Environm Lab, Seattle, WA 98115 USA. [Cornillon, Peter] Univ Rhode Isl, Grad Sch Oceanog, Narragansett, RI 02882 USA. [Weisberg, Robert] Univ S Florida, Coll Marine Sci, St Petersburg, FL 33701 USA. [Barth, Alexander] Univ Liege, Liege, Belgium. [He, Ruoying] N Carolina State Univ, Dept Marine Earth & Atmospher Sci, Raleigh, NC 27695 USA. [Werner, Francisco; Wilkin, John] Rutgers State Univ, Inst Marine & Coastal Sci, New Brunswick, NJ 08903 USA. RP Chassignet, EP (reprint author), Florida State Univ, Ctr Ocean Atmospher Predict Studies, Tallahassee, FL 32306 USA. EM echassignet@coaps.fsu.edu RI Wilkin, John/E-5343-2011; Halliwell, George/B-3046-2011 OI Wilkin, John/0000-0002-5444-9466; Halliwell, George/0000-0003-4216-070X NR 24 TC 119 Z9 125 U1 2 U2 16 PU OCEANOGRAPHY SOC PI ROCKVILLE PA P.O. BOX 1931, ROCKVILLE, MD USA SN 1042-8275 J9 OCEANOGRAPHY JI Oceanography PD JUN PY 2009 VL 22 IS 2 SI SI BP 64 EP 75 DI 10.5670/oceanog.2009 PG 12 WC Oceanography SC Oceanography GA 457WC UT WOS:000266964200013 ER PT J AU Wunsch, C Heimbach, P Ponte, RM Fukumori, I AF Wunsch, Carl Heimbach, Patrick Ponte, Rui M. Fukumori, Ichiro CA ECCO-GODAE Consortium Members TI THE GLOBAL GENERAL CIRCULATION OF THE OCEAN ESTIMATED BY THE ECCO-CONSORTIUM SO OCEANOGRAPHY LA English DT Article ID MERIDIONAL OVERTURNING CIRCULATION; VARIATIONAL DATA ASSIMILATION; SATELLITE ALTIMETRY; STATE ESTIMATION; MODEL; ADJOINT; SEA; CONSTRUCTION; VARIABILITY; SENSITIVITY AB Following on the heels of the World Ocean Circulation Experiment, the Estimating the Circulation and Climate of the Ocean (ECCO) consortium has been directed at making the best possible estimates of ocean circulation and its role in climate. ECCO is combining state-of-the-art ocean general circulation models. with the nearly complete global ocean data sets for 1992 to present. Solutions are now available that adequately fit almost all types of ocean observations and that are, simultaneously, consistent with the model. These solutions are being applied to understanding ocean variability, biological cycles, coastal physics, geodesy, and many other areas. C1 [Wunsch, Carl; Heimbach, Patrick] MIT, Cambridge, MA 02139 USA. [Ponte, Rui M.] Atmospher & Environm Res Inc, Lexington, MA USA. [Fukumori, Ichiro] CALTECH, Jet Prop Lab, Pasadena, CA USA. RP Wunsch, C (reprint author), MIT, 77 Massachusetts Ave, Cambridge, MA 02139 USA. EM cwunsch@mit.edu RI Heimbach, Patrick/K-3530-2013; OI Heimbach, Patrick/0000-0003-3925-6161; Ponte, Rui/0000-0001-7206-6461 NR 61 TC 76 Z9 77 U1 0 U2 14 PU OCEANOGRAPHY SOC PI ROCKVILLE PA P.O. BOX 1931, ROCKVILLE, MD USA SN 1042-8275 J9 OCEANOGRAPHY JI Oceanography PD JUN PY 2009 VL 22 IS 2 SI SI BP 88 EP 103 PG 16 WC Oceanography SC Oceanography GA 457WC UT WOS:000266964200015 ER PT J AU Gao, GJ Lehan, JP Zhang, WW Griesmann, U Soons, JA AF Gao, Guangjun Lehan, John P. Zhang, William W. Griesmann, Ulf Soons, Johannes A. TI Computer-generated hologram cavity interferometry test for large x-ray mirror mandrels: design SO OPTICAL ENGINEERING LA English DT Article DE computer-generated hologram; mandrel; x-ray optics; optical testing; interferometry ID OBLIQUE-INCIDENCE INTERFEROMETER; NON-OPTICAL SURFACES AB A glancing-incidence interferometric test for large x-ray mirror mandrels, using two computer-generated holograms (CGHs), is described. The two CGHs are used to form a double-pass glancing-incidence system. One layout of the CGH-cavity glancing-incidence interferometer is studied and factors relating to its design are analyzed. A semianalytical expression for the phase function is derived that avoids high-order ripple errors and improves the efficiency of the CGH pattern generation. A system of coarse and fine fiducials for establishing the CGH-cavity and aligning the tested mandrel is discussed. Compared with traditional measurement devices, such as coordinate measuring machines (CMMs) or other scanning metrology systems, the CGH-cavity glancing-incidence interferometer can measure a mandrel surface without mechanical contact, at a high spatial sampling frequency, with lower uncertainty, and at high speed. (C) 2009 Society of Photo-Optical Instrumentation Engineers. [DOI: 10.1117/1.3153303] C1 [Gao, Guangjun; Griesmann, Ulf; Soons, Johannes A.] NIST, Mfg Engn Lab, Gaithersburg, MD 20899 USA. [Lehan, John P.; Zhang, William W.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20770 USA. [Lehan, John P.] Univ Maryland, Dept Phys, Baltimore, MD 21250 USA. RP Gao, GJ (reprint author), NIST, Mfg Engn Lab, 100 Bur Dr, Gaithersburg, MD 20899 USA. EM Guangjun.gao@nist.gov FU NASA Goddard Space Flight Center FX The authors would like to thank the Innovative Partnership Program at NASA Goddard Space Flight Center for supporting a portion of this work. NR 16 TC 1 Z9 1 U1 0 U2 0 PU SPIE-SOC PHOTOPTICAL INSTRUMENTATION ENGINEERS PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98225 USA SN 0091-3286 J9 OPT ENG JI Opt. Eng. PD JUN PY 2009 VL 48 IS 6 AR 063602 DI 10.1117/1.3153303 PG 11 WC Optics SC Optics GA 477AE UT WOS:000268487500007 ER PT J AU Burt, EA Taghavi-Larigani, S Tjoelker, RL AF Burt, E. A. Taghavi-Larigani, S. Tjoelker, R. L. TI High-resolution spectroscopy of Hg-201(+) hyperfine structure: A sensitive probe of nuclear structure and the hyperfine anomaly SO PHYSICAL REVIEW A LA English DT Article DE atomic clocks; atomic moments; calibration; error analysis; ground states; hyperfine structure; mercury (metal); nuclear magnetic moment; particle traps; positive ions; statistical analysis ID ION FREQUENCY STANDARD; GROUND-STATE; MERCURY; STABILITY; ISOTOPES; HG+ AB Using Hg-201(+) contained within a linear quadrupole rf ion trap that is part of an atomic clock, we report the results of high-resolution spectroscopy on the hyperfine structure of Hg-201(+). We measure the absolute ground-state hyperfine interval to be 29.954 365 821 130(171)(62)(10) GHz, more than 8 orders of magnitude improvement over the previous measurement. The first error estimate in parentheses is the statistical error in the shifted line center measurement, the second is systematic uncertainty, and the third is calibration uncertainty in the hydrogen maser reference standard. By comparison to the already accurately known ground-state hyperfine interval for Hg-199(+), we are able to derive a value for the hyperfine anomaly in singly ionized mercury, Delta(S-1/2,Hg-199(+),Hg-201(+))=-0.001 625 7(5), now limited by knowledge of the nuclear magnetic-moment ratio. C1 [Burt, E. A.; Taghavi-Larigani, S.; Tjoelker, R. L.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Burt, EA (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. FU National Aeronautics and Space Administration FX The authors gratefully acknowledge helpful discussions with Z.-T. Lu on nuclear structure and to W. Itano on the hyperfine anomaly. This research was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. NR 30 TC 13 Z9 14 U1 1 U2 9 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 2469-9926 EI 2469-9934 J9 PHYS REV A JI Phys. Rev. A PD JUN PY 2009 VL 79 IS 6 AR 062506 DI 10.1103/PhysRevA.79.062506 PG 7 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA 466XZ UT WOS:000267700100069 ER PT J AU Abbott, BP Abbott, R Adhikari, R Ajith, P Allen, B Allen, G Amin, RS Anderson, SB Anderson, WG Arain, MA Araya, M Armandula, H Armor, P Aso, Y Aston, S Aufmuth, P Aulbert, C Babak, S Baker, P Ballmer, S Barker, C Barker, D Barr, B Barriga, P Barsotti, L Barton, MA Bartos, I Bassiri, R Bastarrika, M Behnke, B Benacquista, M Betzwieser, J Beyersdorf, PT Bilenko, IA Billingsley, G Biswas, R Black, E Blackburn, JK Blackburn, L Blair, D Bland, B Bodiya, TP Bogue, L Bork, R Boschi, V Bose, S Brady, PR Braginsky, VB Brau, JE Bridges, DO Brinkmann, M Brooks, AF Brown, DA Brummit, A Brunet, G Bullington, A Buonanno, A Burmeister, O Byer, RL Cadonati, L Camp, JB Cannizzo, J Cannon, KC Cao, J Capano, CD Cardenas, L Caride, S Castaldi, G Caudill, S Cavaglia, M Cepeda, C Chalermsongsak, T Chalkley, E Charlton, P Chatterji, S Chelkowski, S Chen, Y Christensen, N Chung, CTY Clark, D Clark, J Clayton, JH Cokelaer, T Colacino, CN Conte, R Cook, D Corbitt, TRC Cornish, N Coward, D Coyne, DC Creighton, JDE Creighton, TD Cruise, AM Culter, RM Cumming, A Cunningham, L Danilishin, SL Danzmann, K Daudert, B Davies, G Daw, EJ Debra, D Degallaix, J Dergachev, V Desai, S DeSalvo, R Dhurandhar, S Diaz, M Dietz, A Donovan, F Dooley, KL Doomes, EE Drever, RWP Dueck, J Duke, I Dumas, JC Dwyer, JG Echols, C Edgar, M Effler, A Ehrens, P Ely, G Espinoza, E Etzel, T Evans, M Evans, T Fairhurst, S Faltas, Y Fan, Y Fazi, D Fehrmann, H Finn, LS Flasch, K Foley, S Forrest, C Fotopoulos, N Franzen, A Frede, M Frei, M Frei, Z Freise, A Frey, R Fricke, T Fritschel, P Frolov, VV Fyffe, M Galdi, V Garofoli, JA Gholami, I Giaime, JA Giampanis, S Giardina, KD Goda, K Goetz, E Goggin, LM Gonzalez, G Gorodetsky, ML Gossler, S Gouaty, R Grant, A Gras, S Gray, C Gray, M Greenhalgh, RJS Gretarsson, AM Grimaldi, F Grosso, R Grote, H Grunewald, S Guenther, M Gustafson, EK Gustafson, R Hage, B Hallam, JM Hammer, D Hammond, GD Hanna, C Hanson, J Harms, J Harry, GM Harry, IW Harstad, ED Haughian, K Hayama, K Heefner, J Heng, IS Heptonstall, A Hewitson, M Hild, S Hirose, E Hoak, D Hodge, KA Holt, K Hosken, DJ Hough, J Hoyland, D Hughey, B Huttner, SH Ingram, DR Isogai, T Ito, M Ivanov, A Johnson, B Johnson, WW Jones, DI Jones, G Jones, R Ju, L Kalmus, P Kalogera, V Kandhasamy, S Kanner, J Kasprzyk, D Katsavounidis, E Kawabe, K Kawamura, S Kawazoe, F Kells, W Keppel, DG Khalaidovski, A Khalili, FY Khan, R Khazanov, E King, P Kissel, JS Klimenko, S Kokeyama, K Kondrashov, V Kopparapu, R Koranda, S Kozak, D Krishnan, B Kumar, R Kwee, P Laljani, V Lam, PK Landry, M Lantz, B Lazzarini, A Lei, H Lei, M Leindecker, N Leonor, I Li, C Lin, H Lindquist, PE Littenberg, TB Lockerbie, NA Lodhia, D Longo, M Lormand, M Lu, P Lubinski, M Lucianetti, A Luck, H Lundgren, A Machenschalk, B MacInnis, M Mageswaran, M Mailand, K Mandel, I Mandic, V Marka, S Marka, Z Markosyan, A Markowitz, J Maros, E Martin, IW Martin, RM Marx, JN Mason, K Matichard, F Matone, L Matzner, RA Mavalvala, N McCarthy, R McClelland, DE McGuire, SC McHugh, M McIntyre, G McKechan, DJA McKenzie, K Mehmet, M Melatos, A Melissinos, AC Menendez, DF Mendell, G Mercer, RA Meshkov, S Messenger, C Meyer, MS Miller, J Minelli, J Mino, Y Mitrofanov, VP Mitselmakher, G Mittleman, R Miyakawa, O Moe, B Mohanty, SD Mohapatra, SRP Moreno, G Morioka, T Mors, K Mossavi, K MowLowry, C Mueller, G Muller-Ebhardt, H Muhammad, D Mukherjee, S Mukhopadhyay, H Mullavey, A Munch, J Murray, PG Myers, E Myers, J Nash, T Nelson, J Newton, G Nishizawa, A Numata, K O'Dell, J O'Reilly, B O'Shaughnessy, R Ochsner, E Ogin, GH Ottaway, DJ Ottens, RS Overmier, H Owen, BJ Pan, Y Pankow, C Papa, MA Parameshwaraiah, V Patel, P Pedraza, M Penn, S Perraca, A Pierro, V Pinto, IM Pitkin, M Pletsch, HJ Plissi, MV Postiglione, F Principe, M Prix, R Prokhorov, L Punken, O Quetschke, V Raab, FJ Rabeling, DS Radkins, H Raffai, P Raics, Z Rainer, N Rakhmanov, M Raymond, V Reed, CM Reed, T Rehbein, H Reid, S Reitze, DH Riesen, R Riles, K Rivera, B Roberts, P Robertson, NA Robinson, C Robinson, EL Roddy, S Rover, C Rollins, J Romano, JD Romie, JH Rowan, S Rudiger, A Russell, P Ryan, K Sakata, S de la Jordana, LS Sandberg, V Sannibale, V Santamaria, L Saraf, S Sarin, P Sathyaprakash, BS Sato, S Satterthwaite, M Saulson, PR Savage, R Savov, P Scanlan, M Schilling, R Schnabel, R Schofield, R Schulz, B Schutz, BF Schwinberg, P Scott, J Scott, SM Searle, AC Sears, B Seifert, F Sellers, D Sengupta, AS Sergeev, A Shapiro, B Shawhan, P Shoemaker, DH Sibley, A Siemens, X Sigg, D Sinha, S Sintes, AM Slagmolen, BJJ Slutsky, J Smith, JR Smith, MR Smith, ND Somiya, K Sorazu, B Stein, A Stein, LC Steplewski, S Stochino, A Stone, R Strain, KA Strigin, S Stroeer, A Stuver, AL Summerscales, TZ Sun, KX Sung, M Sutton, PJ Szokoly, GP Talukder, D Tang, L Tanner, DB Tarabrin, SP Taylor, JR Taylor, R Thacker, J Thorne, KA Thorne, KS Thuring, A Tokmakov, KV Torres, C Torrie, C Traylor, G Trias, M Ugolini, D Ulmen, J Urbanek, K Vahlbruch, H Vallisneri, M Van Den Broeck, C van der Sluys, MV van Veggel, AA Vass, S Vaulin, R Vecchio, A Veitch, J Veitch, P Veltkamp, C Villar, A Vorvick, C Vyachanin, SP Waldman, SJ Wallace, L Ward, RL Weidner, A Weinert, M Weinstein, AJ Weiss, R Wen, L Wen, S Wette, K Whelan, JT Whitcomb, SE Whiting, BF Wilkinson, C Willems, PA Williams, HR Williams, L Willke, B Wilmut, I Winkelmann, L Winkler, W Wipf, CC Wiseman, AG Woan, G Wooley, R Worden, J Wu, W Yakushin, I Yamamoto, H Yan, Z Yoshida, S Zanolin, M Zhang, J Zhang, L Zhao, C Zotov, N Zucker, ME zur Muhlen, H Zweizig, J AF Abbott, B. P. Abbott, R. Adhikari, R. Ajith, P. Allen, B. Allen, G. Amin, R. S. Anderson, S. B. Anderson, W. G. Arain, M. A. Araya, M. Armandula, H. Armor, P. Aso, Y. Aston, S. Aufmuth, P. Aulbert, C. Babak, S. Baker, P. Ballmer, S. Barker, C. Barker, D. Barr, B. Barriga, P. Barsotti, L. Barton, M. A. Bartos, I. Bassiri, R. Bastarrika, M. Behnke, B. Benacquista, M. Betzwieser, J. Beyersdorf, P. T. Bilenko, I. A. Billingsley, G. Biswas, R. Black, E. Blackburn, J. K. Blackburn, L. Blair, D. Bland, B. Bodiya, T. P. Bogue, L. Bork, R. Boschi, V. Bose, S. Brady, P. R. Braginsky, V. B. Brau, J. E. Bridges, D. O. Brinkmann, M. Brooks, A. F. Brown, D. A. Brummit, A. Brunet, G. Bullington, A. Buonanno, A. Burmeister, O. Byer, R. L. Cadonati, L. Camp, J. B. Cannizzo, J. Cannon, K. C. Cao, J. Capano, C. D. Cardenas, L. Caride, S. Castaldi, G. Caudill, S. Cavaglia, M. Cepeda, C. Chalermsongsak, T. Chalkley, E. Charlton, P. Chatterji, S. Chelkowski, S. Chen, Y. Christensen, N. Chung, C. T. Y. Clark, D. Clark, J. Clayton, J. H. Cokelaer, T. Colacino, C. N. Conte, R. Cook, D. Corbitt, T. R. C. Cornish, N. Coward, D. Coyne, D. C. Creighton, J. D. E. Creighton, T. D. Cruise, A. M. Culter, R. M. Cumming, A. Cunningham, L. Danilishin, S. L. Danzmann, K. Daudert, B. Davies, G. Daw, E. J. Debra, D. Degallaix, J. Dergachev, V. Desai, S. DeSalvo, R. Dhurandhar, S. Diaz, M. Dietz, A. Donovan, F. Dooley, K. L. Doomes, E. E. Drever, R. W. P. Dueck, J. Duke, I. Dumas, J. -C. Dwyer, J. G. Echols, C. Edgar, M. Effler, A. Ehrens, P. Ely, G. Espinoza, E. Etzel, T. Evans, M. Evans, T. Fairhurst, S. Faltas, Y. Fan, Y. Fazi, D. Fehrmann, H. Finn, L. S. Flasch, K. Foley, S. Forrest, C. Fotopoulos, N. Franzen, A. Frede, M. Frei, M. Frei, Z. Freise, A. Frey, R. Fricke, T. Fritschel, P. Frolov, V. V. Fyffe, M. Galdi, V. Garofoli, J. A. Gholami, I. Giaime, J. A. Giampanis, S. Giardina, K. D. Goda, K. Goetz, E. Goggin, L. M. Gonzalez, G. Gorodetsky, M. L. Gossler, S. Gouaty, R. Grant, A. Gras, S. Gray, C. Gray, M. Greenhalgh, R. J. S. Gretarsson, A. M. Grimaldi, F. Grosso, R. Grote, H. Grunewald, S. Guenther, M. Gustafson, E. K. Gustafson, R. Hage, B. Hallam, J. M. Hammer, D. Hammond, G. D. Hanna, C. Hanson, J. Harms, J. Harry, G. M. Harry, I. W. Harstad, E. D. Haughian, K. Hayama, K. Heefner, J. Heng, I. S. Heptonstall, A. Hewitson, M. Hild, S. Hirose, E. Hoak, D. Hodge, K. A. Holt, K. Hosken, D. J. Hough, J. Hoyland, D. Hughey, B. Huttner, S. H. Ingram, D. R. Isogai, T. Ito, M. Ivanov, A. Johnson, B. Johnson, W. W. Jones, D. I. Jones, G. Jones, R. Ju, L. Kalmus, P. Kalogera, V. Kandhasamy, S. Kanner, J. Kasprzyk, D. Katsavounidis, E. Kawabe, K. Kawamura, S. Kawazoe, F. Kells, W. Keppel, D. G. Khalaidovski, A. Khalili, F. Y. Khan, R. Khazanov, E. King, P. Kissel, J. S. Klimenko, S. Kokeyama, K. Kondrashov, V. Kopparapu, R. Koranda, S. Kozak, D. Krishnan, B. Kumar, R. Kwee, P. Laljani, V. Lam, P. K. Landry, M. Lantz, B. Lazzarini, A. Lei, H. Lei, M. Leindecker, N. Leonor, I. Li, C. Lin, H. Lindquist, P. E. Littenberg, T. B. Lockerbie, N. A. Lodhia, D. Longo, M. Lormand, M. Lu, P. Lubinski, M. Lucianetti, A. Lueck, H. Lundgren, A. Machenschalk, B. MacInnis, M. Mageswaran, M. Mailand, K. Mandel, I. Mandic, V. Marka, S. Marka, Z. Markosyan, A. Markowitz, J. Maros, E. Martin, I. W. Martin, R. M. Marx, J. N. Mason, K. Matichard, F. Matone, L. Matzner, R. A. Mavalvala, N. McCarthy, R. McClelland, D. E. McGuire, S. C. McHugh, M. McIntyre, G. McKechan, D. J. A. McKenzie, K. Mehmet, M. Melatos, A. Melissinos, A. C. Menendez, D. F. Mendell, G. Mercer, R. A. Meshkov, S. Messenger, C. Meyer, M. S. Miller, J. Minelli, J. Mino, Y. Mitrofanov, V. P. Mitselmakher, G. Mittleman, R. Miyakawa, O. Moe, B. Mohanty, S. D. Mohapatra, S. R. P. Moreno, G. Morioka, T. Mors, K. Mossavi, K. MowLowry, C. Mueller, G. Mueller-Ebhardt, H. Muhammad, D. Mukherjee, S. Mukhopadhyay, H. Mullavey, A. Munch, J. Murray, P. G. Myers, E. Myers, J. Nash, T. Nelson, J. Newton, G. Nishizawa, A. Numata, K. O'Dell, J. O'Reilly, B. O'Shaughnessy, R. Ochsner, E. Ogin, G. H. Ottaway, D. J. Ottens, R. S. Overmier, H. Owen, B. J. Pan, Y. Pankow, C. Papa, M. A. Parameshwaraiah, V. Patel, P. Pedraza, M. Penn, S. Perraca, A. Pierro, V. Pinto, I. M. Pitkin, M. Pletsch, H. J. Plissi, M. V. Postiglione, F. Principe, M. Prix, R. Prokhorov, L. Punken, O. Quetschke, V. Raab, F. J. Rabeling, D. S. Radkins, H. Raffai, P. Raics, Z. Rainer, N. Rakhmanov, M. Raymond, V. Reed, C. M. Reed, T. Rehbein, H. Reid, S. Reitze, D. H. Riesen, R. Riles, K. Rivera, B. Roberts, P. Robertson, N. A. Robinson, C. Robinson, E. L. Roddy, S. Roever, C. Rollins, J. Romano, J. D. Romie, J. H. Rowan, S. Ruediger, A. Russell, P. Ryan, K. Sakata, S. de la Jordana, L. Sancho Sandberg, V. Sannibale, V. Santamaria, L. Saraf, S. Sarin, P. Sathyaprakash, B. S. Sato, S. Satterthwaite, M. Saulson, P. R. Savage, R. Savov, P. Scanlan, M. Schilling, R. Schnabel, R. Schofield, R. Schulz, B. Schutz, B. F. Schwinberg, P. Scott, J. Scott, S. M. Searle, A. C. Sears, B. Seifert, F. Sellers, D. Sengupta, A. S. Sergeev, A. Shapiro, B. Shawhan, P. Shoemaker, D. H. Sibley, A. Siemens, X. Sigg, D. Sinha, S. Sintes, A. M. Slagmolen, B. J. J. Slutsky, J. Smith, J. R. Smith, M. R. Smith, N. D. Somiya, K. Sorazu, B. Stein, A. Stein, L. C. Steplewski, S. Stochino, A. Stone, R. Strain, K. A. Strigin, S. Stroeer, A. Stuver, A. L. Summerscales, T. Z. Sun, K. -X. Sung, M. Sutton, P. J. Szokoly, G. P. Talukder, D. Tang, L. Tanner, D. B. Tarabrin, S. P. Taylor, J. R. Taylor, R. Thacker, J. Thorne, K. A. Thorne, K. S. Thuering, A. Tokmakov, K. V. Torres, C. Torrie, C. Traylor, G. Trias, M. Ugolini, D. Ulmen, J. Urbanek, K. Vahlbruch, H. Vallisneri, M. Van Den Broeck, C. van der Sluys, M. V. van Veggel, A. A. Vass, S. Vaulin, R. Vecchio, A. Veitch, J. Veitch, P. Veltkamp, C. Villar, A. Vorvick, C. Vyachanin, S. P. Waldman, S. J. Wallace, L. Ward, R. L. Weidner, A. Weinert, M. Weinstein, A. J. Weiss, R. Wen, L. Wen, S. Wette, K. Whelan, J. T. Whitcomb, S. E. Whiting, B. F. Wilkinson, C. Willems, P. A. Williams, H. R. Williams, L. Willke, B. Wilmut, I. Winkelmann, L. Winkler, W. Wipf, C. C. Wiseman, A. G. Woan, G. Wooley, R. Worden, J. Wu, W. Yakushin, I. Yamamoto, H. Yan, Z. Yoshida, S. Zanolin, M. Zhang, J. Zhang, L. Zhao, C. Zotov, N. Zucker, M. E. zur Muehlen, H. Zweizig, J. CA LIGO Sci Collaboration TI Search for gravitational waves from low mass binary coalescences in the first year of LIGO's S5 data SO PHYSICAL REVIEW D LA English DT Article ID INSPIRALLING COMPACT BINARIES; POST-NEWTONIAN ORDER; 2ND-POST-NEWTONIAN ORDER; CONSTRAINING POPULATION; COALESCING BINARIES; SYNTHESIS MODELS; SYSTEMS; RADIATION; CATALOG; FILTERS AB We have searched for gravitational waves from coalescing low mass compact binary systems with a total mass between 2M(circle dot) and 35M(circle dot) and a minimum component mass of 1M(circle dot) using data from the first year of the fifth science run of the three LIGO detectors, operating at design sensitivity. Depending on the mass, we are sensitive to coalescences as far as 150 Mpc from the Earth. No gravitational-wave signals were observed above the expected background. Assuming a population of compact binary objects with a Gaussian mass distribution representing binary neutron star systems, black hole-neutron star binary systems, and binary black hole systems, we calculate the 90% confidence upper limit on the rate of coalescences to be 3.9 X 10(-2) yr(-1)L(10)(-1), 1.1 X 10(-2) yr(-1)L(10)(-1), and 2.5 X 10(-3) yr(-1)L(10)(-1),respectively, where L-10 is 10(10) times the blue solar luminosity. We also set improved upper limits on the rate of compact binary coalescences per unit blue-light luminosity, as a function of mass. C1 [Abbott, B. P.; Abbott, R.; Adhikari, R.; Anderson, S. B.; Araya, M.; Armandula, H.; Aso, Y.; Ballmer, S.; Barton, M. A.; Betzwieser, J.; Billingsley, G.; Black, E.; Blackburn, J. K.; Bork, R.; Boschi, V.; Brooks, A. F.; Cannon, K. C.; Cardenas, L.; Cepeda, C.; Chalermsongsak, T.; Chelkowski, S.; Coyne, D. C.; Daudert, B.; DeSalvo, R.; Echols, C.; Ehrens, P.; Espinoza, E.; Etzel, T.; Fazi, D.; Gustafson, E. K.; Hanna, C.; Heefner, J.; Heptonstall, A.; Hodge, K. A.; Ivanov, A.; Kalmus, P.; Kells, W.; Keppel, D. G.; King, P.; Kondrashov, V.; Kozak, D.; Lazzarini, A.; Lei, M.; Lindquist, P. E.; Mageswaran, M.; Mailand, K.; Maros, E.; Marx, J. N.; McIntyre, G.; Meshkov, S.; Miyakawa, O.; Nash, T.; Ogin, G. H.; Patel, P.; Pedraza, M.; Robertson, N. A.; Russell, P.; Sannibale, V.; Searle, A. C.; Sears, B.; Sengupta, A. S.; Smith, M. R.; Stochino, A.; Taylor, R.; Torrie, C.; Vass, S.; Villar, A.; Wallace, L.; Ward, R. L.; Weinstein, A. J.; Whitcomb, S. E.; Willems, P. A.; Yamamoto, H.; Zhang, L.; Zweizig, J.] CALTECH, LIGO, Pasadena, CA 91125 USA. [Babak, S.; Behnke, B.; Chen, Y.; Gholami, I.; Grunewald, S.; Krishnan, B.; Machenschalk, B.; Papa, M. A.; Robinson, E. L.; Santamaria, L.; Schutz, B. F.; Whelan, J. T.] Max Planck Inst Gravitat Phys, Albert Einstein Inst, D-14476 Golm, Germany. [Ajith, P.; Allen, B.; Aulbert, C.; Brinkmann, M.; Burmeister, O.; Danzmann, K.; Degallaix, J.; Dueck, J.; Fehrmann, H.; Frede, M.; Giampanis, S.; Gossler, S.; Grote, H.; Hewitson, M.; Kawazoe, F.; Khalaidovski, A.; Lueck, H.; Mehmet, M.; Messenger, C.; Mors, K.; Mossavi, K.; Mueller-Ebhardt, H.; Pletsch, H. J.; Prix, R.; Punken, O.; Rainer, N.; Rehbein, H.; Roever, C.; Ruediger, A.; Schilling, R.; Schnabel, R.; Schulz, B.; Seifert, F.; Taylor, J. R.; Veltkamp, C.; Weidner, A.; Weinert, M.; Willke, B.; Winkelmann, L.; Winkler, W.] Max Planck Inst Gravitat Phys, Albert Einstein Inst, D-30167 Hannover, Germany. [Roberts, P.; Summerscales, T. Z.] Andrews Univ, Berrien Springs, MI 49104 USA. [Gray, M.; Grosso, R.; Lam, P. K.; McClelland, D. E.; McKenzie, K.; MowLowry, C.; Mullavey, A.; Rabeling, D. S.; Satterthwaite, M.; Scott, S. M.; Slagmolen, B. J. J.; Wette, K.] Australian Natl Univ, Canberra, ACT 0200, Australia. [Chen, Y.; Li, C.; Mino, Y.; Savov, P.; Somiya, K.; Thorne, K. S.; Vallisneri, M.; Wen, L.] Caltech CaRT, Pasadena, CA 91125 USA. [Clark, J.; Cokelaer, T.; Davies, G.; Dietz, A.; Fairhurst, S.; Harry, I. W.; Jones, G.; McKechan, D. J. A.; Robinson, C.; Sathyaprakash, B. S.; Schutz, B. F.; Sutton, P. J.; Van Den Broeck, C.] Cardiff Univ, Cardiff CF24 3AA, S Glam, Wales. [Christensen, N.; Ely, G.; Isogai, T.] Carleton Coll, Northfield, MN 55057 USA. [Charlton, P.] Charles Sturt Univ, Wagga Wagga, NSW 2678, Australia. [Bartos, I.; Dwyer, J. G.; Khan, R.; Marka, S.; Marka, Z.; Matone, L.; Raics, Z.; Rollins, J.] Columbia Univ, New York, NY 10027 USA. [Gretarsson, A. M.; Zanolin, M.] Embry Riddle Aeronaut Univ, Prescott, AZ 86301 USA. [Colacino, C. N.; Frei, Z.; Raffai, P.; Szokoly, G. P.] Eotvos Lorand Univ, ELTE, H-1053 Budapest, Hungary. [Penn, S.] Hobart & William Smith Coll, Geneva, NY 14456 USA. [Khazanov, E.; Sergeev, A.] Russian Acad Sci, Inst Appl Phys, Nizhnii Novgorod 603950, Russia. 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D.; Haughian, K.; Heng, I. S.; Hough, J.; Huttner, S. H.; Jones, R.; Kumar, R.; Martin, I. W.; Miller, J.; Murray, P. G.; Nelson, J.; Newton, G.; Pitkin, M.; Plissi, M. V.; Reid, S.; Robertson, N. A.; Rowan, S.; Scott, J.; Sorazu, B.; Strain, K. A.; Tokmakov, K. V.; van Veggel, A. A.; Woan, G.] Univ Glasgow, Glasgow G12 8QQ, Lanark, Scotland. [Buonanno, A.; Kanner, J.; Ochsner, E.; Pan, Y.; Shawhan, P.] Univ Maryland, College Pk, MD 20742 USA. [Cadonati, L.; Mohapatra, S. R. P.] Univ Massachusetts, Amherst, MA 01003 USA. [Caride, S.; Dergachev, V.; Goetz, E.; Gustafson, R.; Riles, K.; Zhang, J.] Univ Michigan, Ann Arbor, MI 48109 USA. [Harms, J.; Kandhasamy, S.; Mandic, V.] Univ Minnesota, Minneapolis, MN 55455 USA. [Brau, J. E.; Frey, R.; Harstad, E. D.; Ito, M.; Leonor, I.; Schofield, R.] Univ Oregon, Eugene, OR 97403 USA. [Forrest, C.; Melissinos, A. C.] Univ Rochester, Rochester, NY 14627 USA. [Conte, R.; Postiglione, F.] Univ Salerno, I-84084 Salerno, Italy. [Castaldi, G.; Galdi, V.; Longo, M.; Pierro, V.; Pinto, I. M.; Principe, M.] Univ Sannio Benevento, I-82100 Benevento, Italy. [Jones, D. I.] Univ Southampton, Southampton SO17 1BJ, Hants, England. [Lockerbie, N. A.] Univ Strathclyde, Glasgow G1 1XQ, Lanark, Scotland. [Barriga, P.; Blair, D.; Coward, D.; Dumas, J. -C.; Fan, Y.; Gras, S.; Hoyland, D.; Ju, L.; Wen, L.; Yan, Z.; Zhao, C.] Univ Western Australia, Crawley, WA 6009, Australia. [Allen, B.; Anderson, W. G.; Armor, P.; Biswas, R.; Brady, P. R.; Clayton, J. H.; Creighton, J. D. E.; Flasch, K.; Fotopoulos, N.; Goggin, L. M.; Hammer, D.; Koranda, S.; Mercer, R. A.; Moe, B.; Papa, M. A.; Siemens, X.; Vaulin, R.; Wiseman, A. G.] Univ Wisconsin, Milwaukee, WI 53201 USA. [Bose, S.; Steplewski, S.; Talukder, D.] Washington State Univ, Pullman, WA 99164 USA. RP Abbott, BP (reprint author), CALTECH, LIGO, Pasadena, CA 91125 USA. RI Schutz, Bernard/B-1504-2010; Vyatchanin, Sergey/J-2238-2012; Khazanov, Efim/B-6643-2014; Lucianetti, Antonio/G-7383-2014; Danilishin, Stefan/K-7262-2012; Khalili, Farit/D-8113-2012; Vecchio, Alberto/F-8310-2015; Mow-Lowry, Conor/F-8843-2015; Khan, Rubab/F-9455-2015; Ottaway, David/J-5908-2015; Postiglione, Fabio/O-4744-2015; Sigg, Daniel/I-4308-2015; Pinto, Innocenzo/L-3520-2016; Finn, Lee Samuel/A-3452-2009; Santamaria, Lucia/A-7269-2012; Prokhorov, Leonid/I-2953-2012; Gorodetsky, Michael/C-5938-2008; Strigin, Sergey/I-8337-2012; 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; Pitkin, Matthew/I-3802-2013; Strain, Kenneth/D-5236-2011; Raab, Frederick/E-2222-2011; Martin, Iain/A-2445-2010; Lam, Ping Koy/A-5276-2008; Galdi, Vincenzo/B-1670-2008; Hammond, Giles/B-7861-2009; McClelland, David/E-6765-2010; Lueck, Harald/F-7100-2011; Kawazoe, Fumiko/F-7700-2011; Freise, Andreas/F-8892-2011; Kawabe, Keita/G-9840-2011; Hild, Stefan/A-3864-2010; Rowan, Sheila/E-3032-2010; Hammond, Giles/A-8168-2012; Harms, Jan/J-4359-2012; Bartos, Imre/A-2592-2017; Frey, Raymond/E-2830-2016; Sergeev, Alexander/F-3027-2017; Ward, Robert/I-8032-2014; OI Danilishin, Stefan/0000-0001-7758-7493; Vecchio, Alberto/0000-0002-6254-1617; Khan, Rubab/0000-0001-5100-5168; Postiglione, Fabio/0000-0003-0628-3796; Sigg, Daniel/0000-0003-4606-6526; Finn, Lee Samuel/0000-0002-3937-0688; Gorodetsky, Michael/0000-0002-5159-2742; Allen, Bruce/0000-0003-4285-6256; Zhao, Chunnong/0000-0001-5825-2401; Pitkin, Matthew/0000-0003-4548-526X; Strain, Kenneth/0000-0002-2066-5355; Lam, Ping Koy/0000-0002-4421-601X; Galdi, Vincenzo/0000-0002-4796-3600; McClelland, David/0000-0001-6210-5842; Lueck, Harald/0000-0001-9350-4846; Papa, M.Alessandra/0000-0002-1007-5298; Kanner, Jonah/0000-0001-8115-0577; Aulbert, Carsten/0000-0002-1481-8319; Freise, Andreas/0000-0001-6586-9901; Mandel, Ilya/0000-0002-6134-8946; Whiting, Bernard F/0000-0002-8501-8669; Veitch, John/0000-0002-6508-0713; Principe, Maria/0000-0002-6327-0628; Matichard, Fabrice/0000-0001-8982-8418; Pinto, Innocenzo M./0000-0002-2679-4457; Minelli, Jeff/0000-0002-5330-912X; Santamaria, Lucia/0000-0002-5986-0449; Pierro, Vincenzo/0000-0002-6020-5521; Hallam, Jonathan Mark/0000-0002-7087-0461; Sorazu, Borja/0000-0002-6178-3198; 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; Frey, Raymond/0000-0003-0341-2636; Stein, Leo/0000-0001-7559-9597; Ward, Robert/0000-0001-5503-5241; Whelan, John/0000-0001-5710-6576; LONGO, Maurizio/0000-0001-8325-4003; Fairhurst, Stephen/0000-0001-8480-1961; Boschi, Valerio/0000-0001-8665-2293 FU U.S. National Science Foundation; Science and Technology Facilities Council of the United Kingdom; MaxPlanck-Society; State of Niedersachsen/Germany; Australian Research Council; Council of Scientific and Industrial Research of India; Istituto Nazionale di Fisica Nucleare of Italy; Spanish Ministerio de Educacion y Ciencia; Conselleria d'Economia, Hisenda i Innovacio of the Govern de les Illes Balears; Royal Society; Scottish Funding Council; Scottish Universities Physics Alliance; National Aeronautics and Space Administration; Carnegie Trust; Leverhulme Trust; David and Lucile Packard Foundation; Research Corporation; Alfred P. Sloan Foundation FX The authors thank Marie Anne Bizouard for her time and help in reviewing the accuracy of this research. The authors gratefully acknowledge the support of the U.S. National Science Foundation for the construction and operation of the LIGO Laboratory, and the Science and Technology Facilities Council of the United Kingdom, the MaxPlanck-Society, and the State of Niedersachsen/Germany for support of the construction and operation of the GEO600 detector. The authors also gratefully acknowledge the support of the research by these agencies and by the Australian Research Council, the Council of Scientific and Industrial Research of India, the Istituto Nazionale di Fisica Nucleare of Italy, the Spanish Ministerio de Educacion y Ciencia, the Conselleria d'Economia, Hisenda i Innovacio of the Govern de les Illes Balears, the Royal Society, the Scottish Funding Council, the Scottish Universities Physics Alliance, the National Aeronautics and Space Administration, the Carnegie Trust, the Leverhulme Trust, the David and Lucile Packard Foundation, the Research Corporation, and the Alfred P. Sloan Foundation. NR 53 TC 108 Z9 108 U1 2 U2 19 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 JUN PY 2009 VL 79 IS 12 AR 122001 DI 10.1103/PhysRevD.79.122001 PG 14 WC Astronomy & Astrophysics; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA 466YN UT WOS:000267701500005 ER PT J AU Garofalo, D AF Garofalo, David TI Spacetime constraints on accreting black holes SO PHYSICAL REVIEW D LA English DT Article ID VELOCITY DISPERSION; MASS; LUMINOSITY; DISKS AB We study the spin dependence of accretion onto rotating Kerr black holes using analytic techniques. In its linear regime, angular momentum transport in MHD turbulent accretion flow involves the generation of radial magnetic field connecting plasma in a differentially rotating flow. We take a first principles approach, highlighting the constraint that limits the generation and amplification of radial magnetic fields, stemming from the transfer of energy from mechanical to magnetic form. Because the energy transferred in magnetic form is ultimately constrained by gravitational potential energy or Killing energy, the spin dependence of the latter allows us to derive spin-dependent constraints on the success of the accreting plasma to expel its angular momentum. We find an inverse relationship between this ability and black hole spin. If this radial magnetic field generation forms the basis for angular momentum transfer in accretion flows, accretion rates involving Kerr black holes are expected to be lower as the black hole spin increases in the prograde sense. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Garofalo, D (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM David.A.Garofalo@jpl.nasa.gov FU National Aeronautics and Space Administration; NASA; Oak Ridge Associated Universities FX The research described in this paper was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. D. G. is supported by the NASA Postdoctoral Program at NASA JPL administered by Oak Ridge Associated Universities through contract with NASA. NR 14 TC 0 Z9 0 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 JUN PY 2009 VL 79 IS 12 AR 124036 DI 10.1103/PhysRevD.79.124036 PG 3 WC Astronomy & Astrophysics; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA 466YN UT WOS:000267701500083 ER PT J AU Ghosh, T Saha, R Jain, P Souradeep, T AF Ghosh, Tuhin Saha, Rajib Jain, Pankaj Souradeep, Tarun TI Model independent foreground power spectrum estimation using WMAP 5-year data SO PHYSICAL REVIEW D LA English DT Article ID MICROWAVE-ANISOTROPY-PROBE; COMPONENT SEPARATION; 408 MHZ; EMISSION; SKY; INDEX; MAPS; GHZ; MISSION AB In this paper, we propose and implement on WMAP 5 yr data a model independent approach of foreground power spectrum estimation for multifrequency observations of the CMB experiments. Recently, a model independent approach of CMB power spectrum estimation was proposed by Saha et al. 2006. This methodology demonstrates that the CMB power spectrum can be reliably estimated solely from WMAP data without assuming any template models for the foreground components. In the current paper, we extend this work to estimate the galactic foreground power spectrum using the WMAP 5 yr maps following a self-contained analysis. We apply the model independent method in harmonic basis to estimate the foreground power spectrum and frequency dependence of combined foregrounds. We also study the behavior of synchrotron spectral index variation over different regions of the sky. We use the full sky Haslam map as an external template to increase the degrees of freedom, while computing the synchrotron spectral index over the frequency range from 408 MHz to 94 GHz. We compare our results with those obtained from maximum entropy method foreground maps, which are formed in pixel space. We find that relative to our model independent estimates maximum entropy method maps overestimate the foreground power close to galactic plane and underestimates it at high latitudes. C1 [Ghosh, Tuhin; Saha, Rajib; Souradeep, Tarun] IUCAA, Pune 411007, Maharashtra, India. [Saha, Rajib] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Saha, Rajib] CALTECH, Pasadena, CA 91125 USA. [Saha, Rajib; Jain, Pankaj] Indian Inst Technol, Dept Phys, Kanpur 208016, Uttar Pradesh, India. RP Ghosh, T (reprint author), IUCAA, Post Bag 4, Pune 411007, Maharashtra, India. EM tuhin@iucaa.ernet.in; rajib@caltech.edu; pkjain@iitk.ac.in; tarun@iucaa.ernet.in RI Ghosh, Tuhin/E-6899-2016 FU NASA office of Space Science; Council of Scientific Research and Industrial Research, India FX Computations were carried out on Cetus, the high performance computation facility of IUCAA. Some of the results in this paper used the HEALPIX [22] Package. We acknowledge the use of the Legacy Archive for Microwave Background Data Analysis (LAMBDA). Support for LAMBDA is provided by the NASA office of Space Science. We acknowledge the use of version 1.1 of the Planck reference sky model, prepared by the working group 2 and available at [30]. A portion of the research described in this paper was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. T. G. thanks the Council of Scientific Research and Industrial Research, India for financial support. NR 29 TC 3 Z9 3 U1 0 U2 1 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 JUN PY 2009 VL 79 IS 12 AR 123011 DI 10.1103/PhysRevD.79.123011 PG 11 WC Astronomy & Astrophysics; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA 466YN UT WOS:000267701500017 ER PT J AU Stroeer, A Cannizzo, JK Camp, JB Gagarin, N AF Stroeer, Alexander Cannizzo, John K. Camp, Jordan B. Gagarin, Nicolas TI Methods for detection and characterization of signals in noisy data with the Hilbert-Huang transform SO PHYSICAL REVIEW D LA English DT Article ID EMPIRICAL MODE DECOMPOSITION; TIME-SERIES ANALYSIS; LIGO AB The Hilbert-Huang transform is a novel, adaptive approach to time series analysis that does not make assumptions about the data form. Its adaptive, local character allows the decomposition of nonstationary signals with high time-frequency resolution but also renders it susceptible to degradation from noise. We show that complementing the Hilbert-Huang transform with techniques such as zero-phase filtering, kernel density estimation and Fourier analysis allows it to be used effectively to detect and characterize signals with low signal-to-noise ratios. C1 [Stroeer, Alexander; Cannizzo, John K.; Camp, Jordan B.] NASA, Goddard Space Flight Ctr, Lab Gravitat Phys, Greenbelt, MD 20771 USA. [Gagarin, Nicolas] Starodub Inc, Kensington, MD 20895 USA. [Stroeer, Alexander] Univ Maryland, Dept Astron, CRESST, College Pk, MD 20742 USA. [Cannizzo, John K.] Univ Maryland, Dept Phys, CRESST, Baltimore, MD 21250 USA. RP Stroeer, A (reprint author), NASA, Goddard Space Flight Ctr, Lab Gravitat Phys, Greenbelt, MD 20771 USA. EM Alexander.Stroeer@nasa.gov FU NSF [PHY-0738032] FX We acknowledge helpful comments on this manuscript by Peter Shawhan. This work has been supported in part by NSF Grant No. PHY-0738032. NR 22 TC 4 Z9 4 U1 0 U2 5 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 JUN PY 2009 VL 79 IS 12 AR 124022 DI 10.1103/PhysRevD.79.124022 PG 10 WC Astronomy & Astrophysics; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA 466YN UT WOS:000267701500069 ER PT J AU Zak, M AF Zak, Michail TI Hidden statistics of Schrodinger equation SO PHYSICS ESSAYS LA English DT Article DE Origin of Randomness; Lipchitz Condition; Quantum Potential; Similarity Parameter; Nonquantum-Scale Simulation; Quantum Computing AB Based on the Made lung version of Schrodinger equation, the origin of randomness in quantum mechanics has been traced down to instability generated by quantum potential at the point of departure from a deterministic state. The instability triggered by failure of the Lipchitz condition splits the solution into a continuous set of random samples representing a hidden statistics of Schrodinger equation, i.e., the transitional stochastic process as a "bridge" to quantum world. The hidden statistics confirms the uncertainty principle, and it justifies the belief by most physicists that particle trajectories do not exist, although, to be more precise, it demonstrates that deterministic trajectories exist but they are highly unstable. Unlike the Schrodinger equation that describes probabilities, its hidden statistics simulates probabilities. A dimensionless parameter characterizing the hidden statistics has been introduced. This parameter can be exploited as a similarity criterion, and that allows one to choose an appropriate scale that is not necessarily quantum, for simulation. Following the proposed reinterpretation of quantum formalism, implementation of quantum computing and quantum information processing on a classical scale has been discussed. (C) 2009 Physics Essays Publication. [DOT: 10.4006/1.3123664] C1 CALTECH, Jet Prop Lab, Adv Comp Algorithms & IVHM Grp, Pasadena, CA 91109 USA. RP Zak, M (reprint author), CALTECH, Jet Prop Lab, Adv Comp Algorithms & IVHM Grp, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM michail.zak@gmail.com FU National Aeronautics and Space Administration FX The research described in this paper was performed at Jet Propulsion Laboratory California Institute of Technology under contract with National Aeronautics and Space Administration. NR 10 TC 1 Z9 1 U1 0 U2 0 PU PHYSICS ESSAYS PUBLICATION PI OTTAWA PA PO BOX 8141 STATION T, OTTAWA, ONTARIO K1G 3H6, CANADA SN 0836-1398 J9 PHYS ESSAYS JI Phys. Essays PD JUN PY 2009 VL 22 IS 2 BP 173 EP 178 DI 10.4006/1.3123664 PG 6 WC Physics, Multidisciplinary SC Physics GA V21PU UT WOS:000208220300015 ER PT J AU Bettarini, L Landi, S Velli, M Londrillo, P AF Bettarini, Lapo Landi, Simone Velli, Marco Londrillo, Pasquale TI Three-dimensional evolution of magnetic and velocity shear driven instabilities in a compressible magnetized jet SO PHYSICS OF PLASMAS LA English DT Article DE plasma instability; plasma jets; plasma magnetohydrodynamics; plasma turbulence; vortices ID CURRENT-VORTEX SHEETS; SLOW SOLAR-WIND; SECONDARY INSTABILITY; CORONAL STREAMER; MAGNETOHYDRODYNAMICS; RECONNECTION; SCHEMES; FLOW AB The problem of three-dimensional combined magnetic and velocity shear driven instabilities of a compressible magnetized jet modeled as a plane neutral/current double vortex sheet in the framework of the resistive magnetohydrodynamics is addressed. The resulting dynamics given by the stream+current sheet interaction is analyzed and the effects of a variable geometry of the basic fields are considered. Depending on the basic asymptotic magnetic field configuration, a selection rule of the linear instability modes can be obtained. Hence, the system follows a two-stage path developing either through a fully three-dimensional dynamics with a rapid evolution of kink modes leading to a final turbulent state, or rather through a driving two-dimensional instability pattern that develops on parallel planes on which a reconnection+coalescence process takes place. C1 [Bettarini, Lapo] Katholieke Univ Leuven, Ctr Plasma Astrofys, B-3001 Louvain, Belgium. [Bettarini, Lapo; Landi, Simone; Velli, Marco] Univ Florence, Dipartimento Astron & Sci Spazio, I-50125 Florence, Italy. [Velli, Marco] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Londrillo, Pasquale] INAF Osservatorio Astron Bologna, I-40127 Bologna, Italy. RP Bettarini, L (reprint author), Katholieke Univ Leuven, Ctr Plasma Astrofys, Celestijnenlaan 200B, B-3001 Louvain, Belgium. EM lapo.bettarini@wis.kuleuven.be RI Landi, Simone/G-7282-2015 OI Landi, Simone/0000-0002-1322-8712 NR 30 TC 12 Z9 12 U1 0 U2 4 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 JUN PY 2009 VL 16 IS 6 AR 062302 DI 10.1063/1.3142467 PG 12 WC Physics, Fluids & Plasmas SC Physics GA 465PN UT WOS:000267599400015 ER PT J AU Ryu, CM Ahn, HC Rhee, T Yoon, PH Ziebell, LF Gaelzer, R Vinas, AF AF Ryu, Chang-Mo Ahn, Hee-Chul Rhee, Tongnyeol Yoon, P. H. Ziebell, L. F. Gaelzer, R. Vinas, A. F. TI Simulation of asymmetric solar wind electron distributions SO PHYSICS OF PLASMAS LA English DT Article DE astrophysical plasma; plasma simulation; plasma turbulence; solar wind ID VELOCITY DISTRIBUTION-FUNCTIONS; HELIOS PLASMA-EXPERIMENT; III RADIO-BURSTS; KAPPA-DISTRIBUTIONS; GLOBAL PROCESSES; ENERGY-SPECTRA; SPACE PLASMAS; WAVES; GENERATION; FORESHOCK AB The electron distributions detected in the solar wind feature varying degrees of anisotropic high-energy tail. In a recent work the present authors numerically solved the one-dimensional electrostatic weak turbulence equations by assuming that the solar wind electrons are initially composed of thermal core plus field-aligned counterstreaming beams, and demonstrated that a wide variety of asymmetric energetic tail distribution may result. In the present paper, the essential findings in this work are tested by means of full particle-in-cell simulation technique. It is found that the previous results are largely confirmed, thus providing evidence that the paradigm of local electron acceleration to high-energy tail by self-consistently excited Langmuir turbulence may be relevant to the solar wind environment under certain circumstances. However, some discrepancies are found such that the nearly one-sided energetic tail reported in the numerical solution of the weak turbulence kinetic equation is not shown. C1 [Ryu, Chang-Mo; Ahn, Hee-Chul; Rhee, Tongnyeol] POSTECH, Dept Phys, Pohang, South Korea. [Yoon, P. H.] Massachusetts Technol Lab Inc, Belmont, MA 02478 USA. [Yoon, P. H.] Univ Maryland, IPST, College Pk, MD 20742 USA. [Ziebell, L. F.] Univ Fed Rio Grande do Sul, Inst Fis, Porto Alegre, RS, Brazil. [Gaelzer, R.] Univ Fed Pelotas, Inst Fis & Matemat, Pelotas, RS, Brazil. [Vinas, A. F.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Ryu, CM (reprint author), POSTECH, Dept Phys, Pohang, South Korea. EM ryu201@postech.ac.kr RI Yoon, Peter/E-2395-2013; Ziebell, Luiz/N-7334-2014; Gaelzer, Rudi/E-4437-2013 OI Gaelzer, Rudi/0000-0001-5851-7959 FU Korea Science and Engineering Foundation [R11-2008-07201003-0]; POSCO; Brazilian agencies Conselho Nacional de Desenvolvimento Cientifico e Tecnologico (CNPq); Fundacao de Amparo Pesquisa do Estado do Rio Grande do Sul (FAPERGS); AFOSR [FA9550-07-0053] FX This work was supported by Grant No. R11-2008-07201003-0 of the Korea Science and Engineering Foundation and StSc program by POSCO. Numerical computations were performed with the support from KISTI under the 6th Strategic Supercomputing Applications Support Program. C. M. R. acknowledges the technical support from S. M. Lee of the Supercomputing Center. This work has been partially supported by the Brazilian agencies Conselho Nacional de Desenvolvimento Cientifico e Tecnologico (CNPq) and Fundacao de Amparo Pesquisa do Estado do Rio Grande do Sul (FAPERGS). The research by P. H. Y. was supported by AFOSR under Contract No. FA9550-07-0053. NR 52 TC 5 Z9 5 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 JUN PY 2009 VL 16 IS 6 AR 062902 DI 10.1063/1.3085795 PG 5 WC Physics, Fluids & Plasmas SC Physics GA 465PN UT WOS:000267599400040 ER PT J AU McGuire, PC Bishop, JL Brown, AJ Fraeman, AA Marzo, GA Morgan, MF Murchie, SL Mustard, JF Parente, M Pelkey, SM Roush, TL Seelos, FP Smith, MD Wendt, L Wolff, MJ AF McGuire, Patrick C. Bishop, Janice L. Brown, Adrian J. Fraeman, Abigail A. Marzo, Giuseppe A. Morgan, M. Frank Murchie, Scott L. Mustard, John F. Parente, Mario Pelkey, Shannon M. Roush, Ted L. Seelos, Frank P. Smith, Michael D. Wendt, Lorenz Wolff, Michael J. TI An improvement to the volcano-scan algorithm for atmospheric correction of CRISM and OMEGA spectral data SO PLANETARY AND SPACE SCIENCE LA English DT Article DE Mars; Correction for atmospheric CO2; Hyperspectral imaging; Surface Hydration ID MARS; EXPRESS AB The observations of Mars by the CRISM and OMEGA hyperspectral imaging spectrometers require correction for photometric, atmospheric and thermal effects prior to the interpretation of possible mineralogical features in the spectra. Here, we report on a simple, yet non-trivial, adaptation to the commonly-used volcano-scan correction technique for atmospheric CO2, which allows for the improved detection of minerals with intrinsic absorption bands at wavelengths between 1.9 and 2.1 mu m. This volcano-scan technique removes the absorption bands of CO2 by ensuring that the Lambert albedo is the same at two wavelengths: 1.890 and 2.011 mu m, with the first wavelength outside the CO2 gas bands and the second wavelength deep inside the CO2 gas bands. Our adaptation to the volcano-scan technique moves the first wavelength from 1.890 mu m to be instead within the gas bands at 1.980 mu m, and for CRISM data, cur adaptation shifts the second wavelength slightly, to 2.007 mu m. We also report on our efforts to account for a slight similar to 0.001 mu m shift in wavelengths due to thermal effects in the CRISM instrument. (C) 2009 Elsevier Ltd. All rights reserved. C1 [McGuire, Patrick C.] Washington Univ, McDonnell Ctr Space Sci, St Louis, MO USA. [McGuire, Patrick C.; Wendt, Lorenz] Free Univ Berlin, Dept Planetary Sci & Remote Sensing, D-12249 Berlin, Germany. [Bishop, Janice L.; Brown, Adrian J.; Parente, Mario] SETI Inst, Mountain View, CA USA. [Fraeman, Abigail A.; Mustard, John F.; Pelkey, Shannon M.] Brown Univ, Dept Geol Sci, Providence, RI 02912 USA. [Bishop, Janice L.; Marzo, Giuseppe A.; Roush, Ted L.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Morgan, M. Frank; Murchie, Scott L.; Seelos, Frank P.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD USA. [Smith, Michael D.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Wolff, Michael J.] Space Sci Inst, Boulder, CO USA. RP McGuire, PC (reprint author), Univ Chicago, Dept Geophys Sci, 5734 S Ellis Ave, Chicago, IL 60637 USA. EM mcguirep@uchicago.edu RI Smith, Michael/C-8875-2012; McGuire, Patrick/D-2962-2013; Marzo, Giuseppe/A-9765-2015; Murchie, Scott/E-8030-2015; Morgan, Frank/C-5246-2016; Seelos, Frank/C-7875-2016 OI McGuire, Patrick/0000-0001-6592-4966; Murchie, Scott/0000-0002-1616-8751; Morgan, Frank/0000-0003-3166-7732; Seelos, Frank/0000-0001-9721-941X FU Applied Physics Laboratory [1277793]; German Space Agency (DLR) FX PCM acknowledges support from and conversations with Raymond Arvidson, Gerhard Neukum, Selby Cull, Sandra Wiseman, Kim Lichtenberg, Bethany Ehlmann, Ernst Hauber, Tom Stein, Lars Arvidson, and Margo Mueller. The work by PCM has been funded by a Robert M. Walker senior research fellowship from the McDonnell Center for the Space Sciences and by a Humboldt Research Fellowship. The authors from institutions in the USA acknowledge support from NASA funds through the Applied Physics Laboratory, under subcontract from the jet Propulsion Laboratory through JPL Contract #1277793. LW has been supported by the German Space Agency (DLR) within the Mars Express project. NR 21 TC 81 Z9 81 U1 1 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 JUN PY 2009 VL 57 IS 7 BP 809 EP 815 DI 10.1016/j.pss.2009.03.007 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 459HF UT WOS:000267091500011 ER PT J AU Arridge, CS Gilbert, LK Lewis, GR Sittler, EC Jones, GH Kataria, DO Coates, AJ Young, DT AF Arridge, Christopher S. Gilbert, Linda K. Lewis, Gethyn R. Sittler, Edward C. Jones, Geraint H. Kataria, Dhiren O. Coates, Andrew J. Young, David T. TI The effect of spacecraft radiation sources on electron moments from the Cassini CAPS electron spectrometer SO PLANETARY AND SPACE SCIENCE LA English DT Article DE Cassini; Electrostatic analyser; Penetrating radiation; Moments; Noise subtraction ID PLASMA AB Data from the Cassini plasma spectrometer (CAPS) electron spectrometer (ELS) have been found to be contaminated with an energy-independent background count rate which has been associated with radiation sources on Cassini. In this paper we describe this background radiation and quantitatively assess its impact on numerically integrated electron moments. The general properties of such a background and its effects on numerical moments are derived. The properties of the ELS background are described and a model for the background presented. A model to generate synthetic ELS spectra is presented and used to evaluate the density and temperature of pure noise and then extended to include ambient distributions. It is shown that the presence of noise produces a saturation of the electron density and temperature at quasi-constant values when the instrument is at background, but that these noise level moments are dependent on the floating spacecraft potential and the orientation of the ELS instrument with respect to the spacecraft. When the ambient distribution has a poor signal-to-noise ratio (SNR) the noise determines the density and temperature: however, as the SNR increases (increasing primarily with density) the density and temperature tend to those of the ambient distribution. It is also shown that these noise effects produce highly artificial density-temperature inverse correlations. A method to subtract this noise is presented and shown to correct for the presence of the noise. Simulated error estimates for the density and temperature are also presented. The analysis described in this paper not only applies to weak background noise, but also to more significant penetrating backgrounds such as those in radiation belt regions of planetary magnetospheres. (C) 2009 Elsevier Ltd. All rights reserved. C1 [Arridge, Christopher S.; Gilbert, Linda K.; Lewis, Gethyn R.; Jones, Geraint H.; Kataria, Dhiren O.; Coates, Andrew J.] Univ Coll London, Mullard Space Sci Lab, Dept Space & Climate Phys, Dorking RH5 6NT, Surrey, England. [Arridge, Christopher S.; Gilbert, Linda K.; Lewis, Gethyn R.; Jones, Geraint H.; Coates, Andrew J.] UCL, Ctr Planetary Sci UCL Birkbeck, London WC1E 6BT, England. [Sittler, Edward C.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Young, David T.] SW Res Inst, San Antonio, TX USA. RP Arridge, CS (reprint author), Univ Coll London, Mullard Space Sci Lab, Dept Space & Climate Phys, Holmbury St Mary, Dorking RH5 6NT, Surrey, England. EM chris.arridge@physics.org RI Arridge, Christopher/A-2894-2009; Coates, Andrew/C-2396-2008; Jones, Geraint/C-1682-2008; OI Arridge, Christopher/0000-0002-0431-6526; Coates, Andrew/0000-0002-6185-3125; Jones, Geraint/0000-0002-5859-1136 NR 17 TC 24 Z9 24 U1 0 U2 2 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 JUN PY 2009 VL 57 IS 7 BP 854 EP 869 DI 10.1016/j.pss.2009.02.011 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 459HF UT WOS:000267091500017 ER PT J AU Le Corre, L Le Mouelic, S Sotin, C Combe, JP Rodriguez, S Barnes, JW Brown, RH Buratti, BJ Jaumann, R Soderblom, J Soderblom, LA Clark, R Baines, KH Nicholson, PD AF Le Corre, L. Le Mouelic, S. Sotin, C. Combe, J. -P. Rodriguez, S. Barnes, J. W. Brown, R. H. Buratti, B. J. Jaumann, R. Soderblom, J. Soderblom, L. A. Clark, R. Baines, K. H. Nicholson, P. D. TI Analysis of a cryolava flow-like feature on Titan SO PLANETARY AND SPACE SCIENCE LA English DT Article DE Infrared observations; Radar observations; Infrared spectroscopy; Titan ID HUYGENS LANDING SITE; CASSINI VIMS; OMEGA/MARS EXPRESS; RADAR MAPPER; SURFACE; SPECTROSCOPY; METHANE; ICE; TEMPERATURE; DIVERSITY AB This paper reports on the analysis of the highest spatial resolution hyperspectral images acquired by the Visual and Infrared Mapping Spectrometer (VIMS) onboard the Cassini spacecraft during its prime mission. A bright area matches a flow-like feature coming out of a caldera-like feature observed in Synthetic Aperture Radar (SAR) data recorded by the Cassini radar experiment [Lopes et al., 2007. Cryovolcanic features on Titan's surface as revealed by the Cassini Titan Radar Mapper. Icarus 186, 395-412, doi:10.1016/j.icarus.2006.09.006]. In this SAR image, the flow extends about 160 km east of the caldera. The contrast in brightness between the flow and the surroundings progressively vanishes, suggesting alteration or evolution of the composition of the cryolava during the lifetime of the eruptions. Dunes seem to cover part of this flow on its eastern end. We analyze the different terrains using the Spectral Mixing Analysis (SMA) approach of the Multiple-Endmember Linear Unmixing Model (MELSUM, Combe et al., 2008). The study area can be fully modeled by using only two types of terrains. Then, the VIMS spectra are compared with laboratory spectra of known materials in the relevant atmospheric windows (from 1 to 2.78 mu m). We considered simple molecules that could be produced during cryovolcanic events. including H(2)O, CO(2) (using two different grain sizes), CH(4) and NH(3). We find that the mean spectrum of the cryoflow-like feature is not consistent with pure water ice. It can be best fitted by linear combinations of spectra of the candidate materials, showing that its composition is compatible with a mixture of H(2)O, CH(4) and CO(2). (C) 2009 Elsevier Ltd. All rights reserved. C1 [Le Corre, L.; Le Mouelic, S.] Univ Nantes, CNRS, Lab Planetol & Geodynam, UMR 6112, F-44000 Nantes, France. [Sotin, C.; Buratti, B. J.; Baines, K. H.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Combe, J. -P.] A Columbus Technol & Serv Inc, Bear Fight Ctr, Winthrop, WA 98862 USA. [Barnes, J. W.] Univ Idaho, Dept Phys, Moscow, ID 83844 USA. [Brown, R. H.; Soderblom, J.] Univ Arizona, Lunar & Planetary Lab, Dept Planetary Sci, Tucson, AZ 85721 USA. [Jaumann, R.] DLR, Inst Planetary Res, D-12489 Berlin, Germany. [Soderblom, L. A.] US Geol Survey, Flagstaff, AZ 86001 USA. [Clark, R.] US Geol Survey, Denver Fed Ctr, Denver, CO 80225 USA. [Nicholson, P. D.] Cornell Univ, Dept Astron, Ithaca, NY 14853 USA. RP Le Corre, L (reprint author), Univ Nantes, UFR Sci & Tech, LPGNantes, CNRS,UMR 6112, 2 Rue Houssiniere,BP 92208, F-44322 Nantes, France. EM lucille.le-corre@univ-nantes.fr RI Barnes, Jason/B-1284-2009; Rodriguez, Sebastien/H-5902-2016; OI Barnes, Jason/0000-0002-7755-3530; Rodriguez, Sebastien/0000-0003-1219-0641; Soderblom, Jason/0000-0003-3715-6407; Le Corre, Lucille/0000-0003-0349-7932 FU French Space Agency (CNES) FX The author wish to thank Pascal Rannou for providing the total optical depth of methane in the atmosphere of Titan. The first author would like to thank Nantes Metropole for her Ph.D. grant. Thanks to the VIMS team for getting the data. We also thank T. McCord and G. Hansen for their constructive comments on a previous version of this paper. A part of this work was carried out at JPL under contract with NASA. Support by the French Space Agency (CNES) is greatly appreciated. NR 56 TC 20 Z9 20 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 JUN PY 2009 VL 57 IS 7 BP 870 EP 879 DI 10.1016/j.pss.2009.03.005 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 459HF UT WOS:000267091500018 ER PT J AU Boxe, CS Saiz-Lopez, A AF Boxe, C. S. Saiz-Lopez, A. TI Influence of thin liquid films on polar ice chemistry: Implications for Earth and planetary science SO POLAR SCIENCE LA English DT Article DE Thin liquid films; Quasi-liquid layer (QLL); Planetary science; Snow photochemistry; Ice photochemistry; Soil photochemistry; Brine layer (BL) AB The polar snowpack (and sea-ice) plays a major role in affecting overlying boundary layer chemistry and has only recently come to light. Furthermore, the understanding of this system and its importance is steadily growing. Investigations done thus far, nonetheless, examined the subsets of the polar environment as an uncoupled system. Analogous to some materials, the surface of snow/ice exhibits thin liquid layers (e.g., the quasi-liquid layer (QLL) and brine layer (BL)). This paper gives an overview of thin liquid films and illustrations of their function in Earth science. The impact of such films in polar science (i.e., polar snowpack photochemistry) is discussed within the context of how field data has been elucidated through laboratory data and modeling techniques. Specifically, what laboratory and modeling investigations have revealed about the effect of thin liquid layers on constraining field observations and, more importantly, the physicochemical mechanisms that govern the behavior of trace gases within the snowpack (and sea-ice) and how they are released from the polar snowpack. Current and future impacts of these findings are discussed, along with putative implications of the effect of thin liquid films in planetary science. (C) 2009 Elsevier B.V. and NIPR. All rights reserved. C1 [Boxe, C. S.; Saiz-Lopez, A.] CALTECH, Jet Prop Lab, NASA, Earth & Space Sci Div, Pasadena, CA 91109 USA. RP Boxe, CS (reprint author), CALTECH, Jet Prop Lab, NASA, Earth & Space Sci Div, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM Christopher.Boxe@jpl.nasa.gov RI Saiz-Lopez, Alfonso/B-3759-2015 OI Saiz-Lopez, Alfonso/0000-0002-0060-1581 FU NASA Postdoctoral Program at the Jet Propulsion Laboratory; NASA Upper Atmosphere Research and Tropospheric Chemistry Programs FX C. S. Boxe and A. Saiz-Lopez were supported by an appointment to the NASA Postdoctoral Program at the Jet Propulsion Laboratory, administered by Oak Ridge Associated Universities through a contract with the National Aeronautics and Space Administration (NASA). Research at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with NASA, was supported by the NASA Upper Atmosphere Research and Tropospheric Chemistry Programs. NR 68 TC 7 Z9 7 U1 0 U2 4 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 1873-9652 EI 1876-4428 J9 POLAR SCI JI Polar Sci. PD JUN PY 2009 VL 3 IS 1 BP 73 EP 81 DI 10.1016/j.polar.2009.01.001 PG 9 WC Ecology; Geosciences, Multidisciplinary SC Environmental Sciences & Ecology; Geology GA V33OP UT WOS:000209028400005 ER PT J AU Capo-Lugo, PA Bainum, PM AF Capo-Lugo, P. A. Bainum, P. M. TI Effects of satellite dimensions in the solar pressure formulation for formation flying SO PROCEEDINGS OF THE INSTITUTION OF MECHANICAL ENGINEERS PART G-JOURNAL OF AEROSPACE ENGINEERING LA English DT Article ID BENCHMARK TETRAHEDRON CONSTELLATION; DISTANCE CONSTRAINTS AB In highly elliptical orbits, the solar pressure can perturb the motion of a constellation through the entire orbit because of the longer exposure of the satellites to the Sun. The Tschauner-Hempel equations for a perturbed motion will be used to explain the motion of a pair of satellites about the Earth in a highly elliptical orbit. In this set of equations, the solar pressure formulation will be written differently to determine how the satellite dimensions can affect the control effort to perform the drift correction. To maintain the separation distance constraints, the authors developed a hierarchical control scheme, in discrete format, that takes care of the perturbation effects of the Earth and the Sun. In summary, this article will show how the differences of the satellite dimensions in the solar pressure formulation can cause variations in the control effort. C1 [Capo-Lugo, P. A.] NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35806 USA. [Bainum, P. M.] Howard Univ, Dept Mech Engn, Washington, DC 20059 USA. RP Capo-Lugo, PA (reprint author), NASA, George C Marshall Space Flight Ctr, 685 Providence Main St NW, Huntsville, AL 35806 USA. EM Pedro.A.Capo-Lugo@nasa.gov NR 19 TC 2 Z9 2 U1 0 U2 1 PU PROFESSIONAL ENGINEERING PUBLISHING LTD PI WESTMINISTER PA 1 BIRDCAGE WALK, WESTMINISTER SW1H 9JJ, ENGLAND SN 0954-4100 J9 P I MECH ENG G-J AER JI Proc. Inst. Mech. Eng. Part G-J. Aerosp. Eng. PD JUN PY 2009 VL 223 IS G4 BP 453 EP 463 DI 10.1243/09544100JAERO452 PG 11 WC Engineering, Aerospace; Engineering, Mechanical SC Engineering GA 467FL UT WOS:000267723300014 ER PT J AU Launius, RD AF Launius, Roger D. TI Abandoned in Place: Interpreting the US Material Culture of the Moon Race SO PUBLIC HISTORIAN LA English DT Article DE Apollo program; Kennedy Space Center; Mission Control Center; Apollo Command Modules; Apollo lunar landing sites ID CHALLENGE; MEMORY AB The U.S. space race of the 1960 was an enormous undertaking, costing $25.4 billion (about $125 billion in 2009 dollars) with only the building of the Panama Canal rivalling the Apollo program's size as the largest nonmilitary technological endeavor ever undertaken by the United States. In the process, the United States built a massive infrastructure to support missions to the Moon. In the aftermath of the successful completion of the program, much of this infrastructure was abandoned, some was altered for other uses, and much torn down. This paper surveys six major cultural landmarks of the Moon race, assessing their differing fates: 1. The Apollo Launch Pads-LC 39A and B-Kennedy Space Center, Florida. 2. The Vertical Assembly Building (VAB), Kennedy Space Center, Florida. 3. Mission Control Center (MCC), Johnson Space Center, Houston, Texas. 4. Six Apollo landing sites on the Moon. 5. Lunar Landing Research Facility, Langley Research Center, Hampton, Virginia. 6. Apollo Command Modules on display in various museums around the nation, and in London. C1 [Launius, Roger D.] Smithsonian Inst, Natl Air & Space Museum, Div Space Hist, Washington, DC 20560 USA. [Launius, Roger D.] NASA, Washington, DC USA. RP Launius, RD (reprint author), Smithsonian Inst, Natl Air & Space Museum, Div Space Hist, Washington, DC 20560 USA. NR 91 TC 0 Z9 0 U1 3 U2 7 PU UNIV CALIFORNIA PRESS PI BERKELEY PA C/O JOURNALS DIVISION, 2000 CENTER ST, STE 303, BERKELEY, CA 94704-1223 USA SN 0272-3433 J9 PUBL HISTORIAN JI Public Hist. PD SUM PY 2009 VL 31 IS 3 BP 9 EP 38 DI 10.1525/tph.2009.31.3.9 PG 30 WC History SC History GA 492YL UT WOS:000269698700002 ER PT J AU Armus, L Mazzarella, JM Evans, AS Surace, JA Sanders, DB Iwasawa, K Frayer, DT Howell, JH Chan, B Petric, A Vavilkin, T Kim, DC Haan, S Inami, H Murphy, EJ Appleton, PN Barnes, JE Bothun, G Bridge, CR Charmandaris, V Jensen, JB Kewley, LJ Lord, S Madore, BF Marshall, JA Melbourne, JE Rich, J Satyapal, S Schulz, B Spoon, HWW Sturm, E Veilleux, S Xu, K AF Armus, L. Mazzarella, J. M. Evans, A. S. Surace, J. A. Sanders, D. B. Iwasawa, K. Frayer, D. T. Howell, J. H. Chan, B. Petric, A. Vavilkin, T. Kim, D. C. Haan, S. Inami, H. Murphy, E. J. Appleton, P. N. Barnes, J. E. Bothun, G. Bridge, C. R. Charmandaris, V. Jensen, J. B. Kewley, L. J. Lord, S. Madore, B. F. Marshall, J. A. Melbourne, J. E. Rich, J. Satyapal, S. Schulz, B. Spoon, H. W. W. Sturm, E. Veilleux, S. Xu, K. TI GOALS: The Great Observatories All-Sky LIRG Survey SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF THE PACIFIC LA English DT Article ID ULTRALUMINOUS INFRARED GALAXIES; SPITZER-SPACE-TELESCOPE; STAR-FORMATION RATE; FORMATION RATE INDICATOR; ACTIVE GALACTIC NUCLEUS; K-BAND SPECTROSCOPY; RESOLUTION X-RAY; 2 JY SAMPLE; OPTICAL SPECTROSCOPY; ANTENNAE GALAXIES AB The Great Observatories All-Sky LIRG Survey (GOALS(20)) combines data from NASA's Spitzer Space Telescope, Chandra X-Ray Observatory, Hubble Space Telescope (HST), and Galaxy Evolution Explorer (GALEX) observatories, together with ground-based data, into a comprehensive imaging and spectroscopic survey of over 200 low-redshift (z < 0.088), Luminous Infrared Galaxies (LIRGs). The LIRGs are a complete subset of the IRAS Revised Bright Galaxy Sample (RBGS), which comprises 629 extragalactic objects with 60 mu m flux densities above 5.24 Jy, and Galactic latitudes above five degrees. The LIRGs targeted in GOALS span the full range of nuclear spectral types defined via traditional optical line-ratio diagrams (type-1 and type-2 AGN, LINERs, and starbursts) as well as interaction stages (major mergers, minor mergers, and isolated galaxies). They provide an unbiased picture of the processes responsible for enhanced infrared emission in galaxies in the local Universe. As an example of the analytic power of the multiwavelength GOALS data set, we present Spitzer, Chandra, HST, and GALEX images and spectra for the interacting system VV 340 (IRAS F14547 + 2449). The Spitzer MIPS imaging data indicates that between 80-95% of the total far-infrared emission (or about 5 x 10(11) L(circle dot)) originates in VV 340 north. While the Spitzer IRAC colors of VV 340 north and south are consistent with star-forming galaxies, both the Spitzer IRS and Chandra ACIS data indicate the presence of an AGN in VV 340 north. The observed line fluxes, without correction for extinction, imply that the AGN accounts for less than 10%-20% of the observed infrared emission. The X-ray data are consistent with a heavily absorbed (N(H) >= 10(24) cm(-2)) AGN. The GALEX far and near-UV fluxes imply a extremely large infrared "excess" (IRX) for the system (F(IR)/F(fuv) similar to 81) which is well above the correlation seen in starburst galaxies. Most of this excess is driven by VV 340 N, which has an IR excess of nearly 400. The VV 340 system seems to be comprised of two very different galaxies: an infrared luminous edge-on galaxy (VV 340 north) that dominates the long-wavelength emission from the system, which hosts a buried AGN; and a face-on starburst (VV 340 south) that dominates the short-wavelength emission. C1 [Armus, L.; Surace, J. A.; Howell, J. H.; Petric, A.; Haan, S.; Murphy, E. J.; Bridge, C. R.] CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA. [Mazzarella, J. M.; Chan, B.; Lord, S.] CALTECH, Ctr Infrared Proc & Anal, Pasadena, CA 91125 USA. [Evans, A. S.; Kim, D. C.] Natl Radio Astron Observ, Charlottesville, VA 22903 USA. [Evans, A. S.] Univ Virginia, Dept Astron, Charlottesville, VA 22904 USA. [Sanders, D. B.; Barnes, J. E.; Kewley, L. J.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. [Iwasawa, K.] INAF Observ Astron Bologna, Bologna, Italy. [Frayer, D. T.; Appleton, P. N.; Xu, K.] CALTECH, NASA Herschel Sci Ctr, Pasadena, CA 91125 USA. [Vavilkin, T.] SUNY Stony Brook, Dept Phys & Astron, Stony Brook, NY 11794 USA. [Bothun, G.] Univ Oregon, Dept Phys, Eugene, OR 97402 USA. [Charmandaris, V.] Univ Crete, Dept Phys, GR-71003 Iraklion, Greece. [Jensen, J. B.] Gemini Observ, Tucson, AZ 85719 USA. [Madore, B. F.] Observ Carnegie Inst Washington, Pasadena, CA 91101 USA. [Marshall, J. A.] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. [Satyapal, S.] George Mason Univ, Dept Phys & Astron, Fairfax, VA 22030 USA. [Spoon, H. W. W.] Cornell Univ, Dept Astron, Ithaca, NY 14953 USA. [Sturm, E.] MPE, D-85741 Garching, Germany. [Veilleux, S.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. RP Armus, L (reprint author), CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA. RI Charmandaris, Vassilis/A-7196-2008; OI Charmandaris, Vassilis/0000-0002-2688-1956; Rich, Jeffrey/0000-0002-5807-5078; Appleton, Philip/0000-0002-7607-8766 FU NASA [NAS5-98034, HST-GO10592.01-A, HST-GO11196.01-A]; NSF [AST 02-06262] FX The Spitzer Space Telescope is operated by the Jet Propulsion Laboratory, California Institute of Technology, under NASA contract 1407. This research has made use of the NASA/IPAC Extragalactic Database (NED) which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. Based on observations made with the NASA Galaxy Evolution Explorer. GALEX is operated for NASA by the California Institute of Technology under NASA contract NAS5-98034. TV, ASE, and DCK were supported by NSF grant AST 02-06262 and by NASA through grants HST-GO10592.01-A and HST-GO11196.01-A from the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy under NASA contract NR 94 TC 134 Z9 134 U1 0 U2 3 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 JUN PY 2009 VL 121 IS 880 BP 559 EP 576 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 456FL UT WOS:000266827100001 ER PT J AU Wesley, WR Simpson, JR Parker, PA Pignatiello, JJ AF Wesley, Wayne R. Simpson, James R. Parker, Peter A. Pignatiello, Joseph J., Jr. TI Prediction Variance and G-Criterion Location for Split-Plot Designs SO QUALITY AND RELIABILITY ENGINEERING INTERNATIONAL LA English DT Review DE prediction variance; split-plot designs; design optimality; response surface designs; G-criterion ID RESPONSE-SURFACE DESIGNS; CAPABILITY; FRACTION; SPACE AB Prediction variance properties for completely randomized designs (CRD) are fairly well covered in the response surface literature for both spherical and cuboidal designs. This paper evaluates the impact of changes in the variance ratio on the prediction properties of second-order split-plot designs (SPD). It is shown that the variance ratio not only influences the value of the G-criterion but also its location, in contrast with the G-criterion tendencies in CRD. An analytical method, rather than a heuristic optimization algorithm, is used to compute the prediction variance properties, which include the maximum, minimum and integrated variances for second-order SPD. The analytical equations are functions of the design parameters, radius and variance ratio. As a result, the exact values for these quantities are reported along with the location of the maximum prediction variance used in the G-criterion. The two design spaces of the whole plot and the subplot are studied and as a result, relative efficiency values for these distinct spaces are suggested. Copyright (C) 2008 John Wiley & Sons, Ltd. C1 [Wesley, Wayne R.] Univ Technol, Sch Engn, Kingston 6, Jamaica. [Simpson, James R.; Pignatiello, Joseph J., Jr.] Florida State Univ, Dept Ind & Mfg Engn, Tallahassee, FL 32310 USA. [Parker, Peter A.] NASA, Langley Res Ctr, Hampton, VA 23681 USA. RP Wesley, WR (reprint author), Univ Technol, Sch Engn, 237 Old Hope Rd, Kingston 6, Jamaica. EM wwesley@utech.edu.jm NR 8 TC 1 Z9 1 U1 0 U2 0 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 JUN PY 2009 VL 25 IS 4 BP 381 EP 395 DI 10.1002/qre.975 PG 15 WC Engineering, Multidisciplinary; Engineering, Industrial; Operations Research & Management Science SC Engineering; Operations Research & Management Science GA 453LN UT WOS:000266612100002 ER PT J AU Echternach, PM Schneiderman, JF Shaw, MD Delsing, P AF Echternach, Pierre M. Schneiderman, J. F. Shaw, Matthew D. Delsing, Per TI Progress in the development of a single Cooper-pair box qubit SO QUANTUM INFORMATION PROCESSING LA English DT Article DE Single Cooper-pair box; Qubit; RF-SET; Quantum capacitance ID CHARGE QUBITS; JOSEPHSON-JUNCTIONS; ELECTRON-TRANSISTOR; CIRCUIT AB We describe in this review progress in techniques for measuring the quantum states of the single Cooper-pair box (SCB) at the Jet Propulsion Laboratory, and the use of these techniques to characterize their performance as quantum bits. Initially, the Radio-Frequency-Single-Electron Transistor was used to measure conventional and differential versions of the SCB. To overcome some of the difficulties associated with the radio-frequency single-electron transistor, a transition was made to readout based on the quantum capacitance technique. Using this method, entanglement between two SCBs was demonstrated spectroscopically and with ground state characterization. C1 [Echternach, Pierre M.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Schneiderman, J. F.; Delsing, Per] Chalmers Univ Technol Microtechnol & Nanosci, S-41296 Gothenburg, Sweden. [Shaw, Matthew D.] Univ So Calif, Dept Phys & Astron, Los Angeles, CA 90089 USA. RP Echternach, PM (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. EM pierre.m.echternach@jpl.nasa.gov; justin.schneiderman@chalmers.se; shawm@usc.edu; per.delsing@chalmers.se RI Delsing, Per/F-7288-2010; Schneiderman, Justin/D-4508-2013 OI Delsing, Per/0000-0002-1222-3506; Schneiderman, Justin/0000-0002-4441-2360 FU Jet Propulsion Laboratory, California Institute of Technology; National Aeronautics and Space Administration (NASA); National Security Agency FX We would like to thank Ben Palmer, and Juan Bueno for ongoing assistance. This work was conducted at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration (NASA), and was funded by a grant from the National Security Agency. NR 34 TC 1 Z9 1 U1 1 U2 3 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 1570-0755 J9 QUANTUM INF PROCESS JI Quantum Inf. Process. PD JUN PY 2009 VL 8 IS 2-3 BP 183 EP 198 DI 10.1007/s11128-009-0097-x PG 16 WC Physics, Multidisciplinary; Physics, Mathematical SC Physics GA 420CS UT WOS:000264266600008 ER PT J AU George, KA Hada, M Jackson, LJ Elliott, T Kawata, T Pluth, JM Cucinotta, FA AF George, Kerry A. Hada, Megumi Jackson, Lori J. Elliott, Todd Kawata, Tetsuya Pluth, Janice M. Cucinotta, Francis A. TI Dose Response of gamma Rays and Iron Nuclei for Induction of Chromosomal Aberrations in Normal and Repair-Deficient Cell Lines SO RADIATION RESEARCH LA English DT Article ID DOUBLE-STRAND BREAK; IN-SITU HYBRIDIZATION; INDUCED EXCHANGE ABERRATIONS; ATAXIA-TELANGIECTASIA CELLS; DEPENDENT PROTEIN-KINASE; DNA-DAMAGE; HUMAN-LYMPHOCYTES; SPACE EXPLORATION; MAMMALIAN-CELLS; HEAVY-IONS AB We studied the effects of DNA double-strand break (DSB) repair deficiencies on chromosomal aberration frequency using low doses (<1 Gy) of gamma rays and high-energy iron ions (LET = 151 keV/mu m). Chromosomal aberrations were measured using the fluorescence whole-chromosome painting technique. The cell lines included fibroblasts deficient in ATM (product of the gene that is mutated in ataxia telangiectasia patients) or NBS (product of the gene mutated in the Nijmegen breakage syndrome) and gliomablastoma cells proficient in or lacking DNA-dependent protein kinase (DNA-PK) activity. The yields of both simple and complex chromosomal aberrations were increased in DSB repair-defective cells compared to normal cells; the increase was more than twofold higher for gamma rays compared to iron nuclei. For gamma-ray-induced aberrations, the ATM- and NBS-defective lines were found to have significantly larger quadratic components compared to normal fibroblasts for both simple and complex aberrations, while the linear dose-response term was significantly higher only for the NBS cells. For simple and complex aberrations induced by iron nuclei, regression models preferred purely linear and quadratic dose responses, respectively, for each cell line studied. RBEs were reduced relative to normal cells for all of the DSB repair-defective lines, with the DNA-PK-deficient cells found to have RBEs near unity. The large increase in the quadratic dose-response terms in the DSB repair-deficient cell lines points to the importance of the functions of ATM and NBS in chromatin modifications to facilitate correct DSB repair and to minimize aberration formation. The differences found between AT and NBS cells at lower doses suggest important questions about the applicability of observations of radiation sensitivity at high doses to low-dose exposures. (C) 2009 by Radiation Research Society C1 [Cucinotta, Francis A.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. [George, Kerry A.; Elliott, Todd] Wyle, Houston, TX 77058 USA. [Hada, Megumi; Jackson, Lori J.] USRA Div Life Sci, Houston, TX 77058 USA. [Kawata, Tetsuya] Chiba Univ, Dept Radiol, Grad Sch Med, Chiba, Japan. [Pluth, Janice M.] Univ Calif Berkeley, Lawrence Berkeley Lab, Div Life Sci, Berkeley, CA 94720 USA. RP Cucinotta, FA (reprint author), NASA, Lyndon B Johnson Space Ctr, 2101 NASA Pkwy, Houston, TX 77058 USA. EM Francis.A.Cucinotta@nasa.gov FU U.S. DOE [DE-A103-05ER64088]; NASA [03-OBPR-07-0032-0027] FX We gratefully acknowledge partial financial support provided by the U.S. DOE (DE-A103-05ER64088) and the NASA Space Radiation Program (03-OBPR-07-0032-0027). NR 46 TC 21 Z9 22 U1 0 U2 3 PU RADIATION RESEARCH SOC PI LAWRENCE PA 810 E TENTH STREET, LAWRENCE, KS 66044 USA SN 0033-7587 J9 RADIAT RES JI Radiat. Res. PD JUN PY 2009 VL 171 IS 6 BP 752 EP 763 DI 10.1667/RR1680.1 PG 12 WC Biology; Biophysics; Radiology, Nuclear Medicine & Medical Imaging SC Life Sciences & Biomedicine - Other Topics; Biophysics; Radiology, Nuclear Medicine & Medical Imaging GA 456HN UT WOS:000266835200013 PM 19580482 ER PT J AU Shastry, R Hofer, RR Reid, BM Gallimore, AD AF Shastry, Rohit Hofer, Richard R. Reid, Bryan M. Gallimore, Alec D. TI Method for analyzing ExB probe spectra from Hall thruster plumes SO REVIEW OF SCIENTIFIC INSTRUMENTS LA English DT Article DE charge exchange; plasma collision processes; plasma devices; plasma probes; plasma transport processes AB Various methods for accurately determining ion species' current fractions using ExB probes in Hall thruster plumes are investigated. The effects of peak broadening and charge exchange on the calculated values of current fractions are quantified in order to determine the importance of accounting for them in the analysis. It is shown that both peak broadening and charge exchange have a significant effect on the calculated current fractions over a variety of operating conditions, especially at operating pressures exceeding 10(-5) torr. However, these effects can be accounted for using a simple approximation for the velocity distribution function and a one-dimensional charge exchange correction model. In order to keep plume attenuation from charge exchange below 30%, it is recommended that pz < 2, where p is the measured facility pressure in units of 10(-5) torr and z is the distance from the thruster exit plane to the probe inlet in meters. The spatial variation of the current fractions in the plume of a Hall thruster and the error induced from taking a single-point measurement are also briefly discussed. C1 [Shastry, Rohit; Hofer, Richard R.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Reid, Bryan M.; Gallimore, Alec D.] Univ Michigan, Plasmadynam & Elect Prop Lab, Ann Arbor, MI 48109 USA. RP Shastry, R (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. FU National Aeronautics and Space Administration FX The authors would like to thank John Anderson and Ira Katz at JPL for their assistance on formulation and development of the charge exchange correction model used in this paper, along with Rainer Dressler at Hanscom AFB for providing additional xenon charge exchange cross sections. The research described in this paper was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. The leading author is supported under the Graduate Student Research Program through the National Aeronautics and Space Administration. NR 22 TC 11 Z9 11 U1 0 U2 7 PU AMER INST PHYSICS PI MELVILLE PA CIRCULATION & FULFILLMENT DIV, 2 HUNTINGTON QUADRANGLE, STE 1 N O 1, MELVILLE, NY 11747-4501 USA SN 0034-6748 J9 REV SCI INSTRUM JI Rev. Sci. Instrum. PD JUN PY 2009 VL 80 IS 6 AR 063502 DI 10.1063/1.3152218 PG 11 WC Instruments & Instrumentation; Physics, Applied SC Instruments & Instrumentation; Physics GA 465PZ UT WOS:000267600600013 PM 19566202 ER PT J AU Juckett, DA Wolff, CL AF Juckett, David A. Wolff, Charles L. TI Correspondence between Solar Variability (0.6-aEuro parts per thousand 7.0 Years) and the Theoretical Positions of Rotating Sets of Coupled g Modes SO SOLAR PHYSICS LA English DT Article DE Sunspots; g modes; Solar interior; Rotation; Solar cycle; Solar activity; Spherical harmonics; Stackplots ID SHORT-TERM PERIODICITIES; NORTH-SOUTH ASYMMETRY; DIFFERENTIAL ROTATION; GEOMAGNETIC-ACTIVITY; SUNSPOT ACTIVITY; MAGNETIC-FIELD; OSCILLATIONS; PATTERNS; PERSISTENCE; INDEXES AB Recently, Juckett and Wolff (Solar Phys. 252, 247, 2008) showed that the timing and longitude of sunspot patterns has some correspondence with a model based on coupled g modes. The model maximizes the nonlinear coupling of those g modes sharing harmonic degree a"" to generate a "set(a"")" that assists its own excitation by locally enhancing nuclear burning. Each set(a"") has oscillatory power concentrated at two longitudes, on opposite sides of the Sun and drifts slowly retrograde within the radiative zone (RZ) at a rate that depends on a"". When the strong longitudes of two or more sets overlap, wave dissipation adds extra energy to that locality at the base of the convective envelope increasing convection and then sunspot activity. We compare the main subdecadal sunspot frequencies with the intersections of sets derived from a""=2 -aEuro parts per thousand 11 and G, where G represents unresolvable high-a"" modes that rotate similarly to the RZ. After determining the set(a"") spatial phases, we show that 17 subdecadal oscillations with periods in the range 0.6 to 7.0 years (4.5 to 50 nHz), generated by 23 unique intersections of the 11 sets, are synchronous with 17 corresponding frequencies in the sunspot time series. After optimizing parameters, we find a mean correlation of 0.96 for synchrony among the 17 waveform pairs. These 17 frequencies constitute the bulk of the non-noise subdecadal frequency domain of the sunspot variation. We conclude that the sunspot series contains oscillatory components with the same temporal phases and frequencies as various set(a"") intersections spanning the past a parts per thousand aEuro parts per thousand 100 years. This additional evidence for the role of coupled g modes in sunspot dynamics suggests that more of sunspot variability can be understood with nonmagnetic fluid mechanics than popularly thought. C1 [Juckett, David A.] Michigan State Univ, Dept Chem, E Lansing, MI 48824 USA. [Juckett, David A.] Barros Res Inst, Holt, MI USA. [Wolff, Charles L.] NASA Goddard Space Flight Ctr, Greenbelt, MD USA. RP Juckett, DA (reprint author), Michigan State Univ, Dept Chem, E Lansing, MI 48824 USA. EM juckett@msu.edu; charles.l.wolff@nasa.gov FU Barros Research Institute and Michigan State University FX D.J. is supported by a joint research agreement between Barros Research Institute and Michigan State University. NR 25 TC 1 Z9 1 U1 0 U2 0 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0038-0938 J9 SOL PHYS JI Sol. Phys. PD JUN PY 2009 VL 257 IS 1 BP 13 EP 36 DI 10.1007/s11207-009-9340-y PG 24 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 447CC UT WOS:000266168200002 ER PT J AU Kirk, MS Pesnell, WD Young, CA Webber, SAH AF Kirk, M. S. Pesnell, W. D. Young, C. A. Webber, S. A. Hess TI Automated detection of EUV Polar Coronal Holes during Solar Cycle 23 SO SOLAR PHYSICS LA English DT Article DE Coronal holes; Solar cycle, observations ID SUN AB A new method for automated detection of polar coronal holes is presented. This method, called perimeter tracing, uses a series of 171, 195, and 304 A... full disk images from the Extreme ultraviolet Imaging Telescope (EIT) on SOHO over solar cycle 23 to measure the perimeter of polar coronal holes as they appear on the limbs. Perimeter tracing minimizes line-of-sight obscurations caused by the emitting plasma of the various wavelengths by taking measurements at the solar limb. Perimeter tracing also allows for the polar rotation period to emerge organically from the data as 33 days. We have called this the Harvey rotation rate and count Harvey rotations starting 4 January 1900. From the measured perimeter, we are then able to fit a curve to the data and derive an area within the line of best fit. We observe the area of the northern polar hole area in 1996, at the beginning of solar cycle 23, to be about 4.2% of the total solar surface area and about 3.6% in 2007. The area of the southern polar hole is observed to be about 4.0% in 1996 and about 3.4% in 2007. Thus, both the north and south polar hole areas are no more than 15% smaller now than they were at the beginning of cycle 23. This compares to the polar magnetic field measured to be about 40% less now than it was a cycle ago. C1 [Kirk, M. S.; Pesnell, W. D.; Young, C. A.] ADNET Syst Inc, NASA Goddard Space Flight Ctr, Greenbelt, MD USA. [Webber, S. A. Hess] Catholic Univ Amer, Washington, DC 20064 USA. RP Pesnell, WD (reprint author), ADNET Syst Inc, NASA Goddard Space Flight Ctr, Greenbelt, MD USA. EM mskirk@nmsu.edu; william.d.pesnell@nasa.gov; c.alex.young@nasa.gov; hesssh01@gettysburg.edu RI Pesnell, William/D-1062-2012; OI Pesnell, William/0000-0002-8306-2500; Hess Webber, Shea A/0000-0002-3631-6491 FU NASA FX This work was supported by NASA's Solar Dynamics Observatory (SDO). The EIT images are courtesy of the SOHO/EIT consortium. The referenced SolarSoft software can be found at www.lmsal.com/solarsoft/. NR 22 TC 47 Z9 47 U1 0 U2 0 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0038-0938 J9 SOL PHYS JI Sol. Phys. PD JUN PY 2009 VL 257 IS 1 BP 99 EP 112 DI 10.1007/s11207-009-9369-y PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 447CC UT WOS:000266168200008 ER PT J AU Yan, WZ Li, JC Coebel, KF AF Yan, W. Z. Li, J. C. Coebel, K. F. TI On improving performance of aircraft engine gas path fault diagnosis SO TRANSACTIONS OF THE INSTITUTE OF MEASUREMENT AND CONTROL LA English DT Article DE aircraft engines; classification; classifier fusion; diagnostics; gas path diagnosis; multiple classifier systems; neural networks; support vector machine ID CLASSIFICATION; NETWORKS AB Aircraft engine fault diagnosis plays a crucial role in cost-effective operations of aircraft engines. However, designing in engine fault diagnostic system with the desired performance is a challenging task, because of several characteristics associated with aircraft engines. Geared towards achieving the highest possible performance of fault diagnosis, this paper explores strategies on improving diagnosis performance. Specifically, we introduce flight regime mapping and a two-level multiple classifier system as mean,, to improve classification performance. By designing a real-world aircraft fault diagnostic system, we demonstrate that the strategies adopted in this Study are effective in improving the performance of aircraft engine fault diagnostic systems. C1 [Yan, W. Z.] GE Global Res Ctr, Ind Artificial Intelligence Lab, Niskayuna, NY 12309 USA. [Li, J. C.] Rensselaer Polytech Inst, Dept MANE, Troy, NY 12181 USA. [Coebel, K. F.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Yan, WZ (reprint author), GE Global Res Ctr, Ind Artificial Intelligence Lab, Niskayuna, NY 12309 USA. EM yan@crd.ge.com NR 24 TC 2 Z9 2 U1 1 U2 3 PU SAGE PUBLICATIONS LTD PI LONDON PA 1 OLIVERS YARD, 55 CITY ROAD, LONDON EC1Y 1SP, ENGLAND SN 0142-3312 J9 T I MEAS CONTROL JI Trans. Inst. Meas. Control PD JUN-AUG PY 2009 VL 31 IS 3-4 BP 275 EP 291 DI 10.1177/0142331208092029 PG 17 WC Automation & Control Systems; Instruments & Instrumentation SC Automation & Control Systems; Instruments & Instrumentation GA 472TD UT WOS:000268154200004 ER PT J AU Saha, B Goebel, K Christophersen, J AF Saha, Bhaskar Goebel, Kai Christophersen, Jon TI Comparison of prognostic algorithms for estimating remaining useful life of batteries SO TRANSACTIONS OF THE INSTITUTE OF MEASUREMENT AND CONTROL LA English DT Article DE autoregressive integrated moving average; battery prognostics; extended Kalman filtering; particle filter; relevance vector machine; remaining useful life; uncertainty management ID HYBRID-ELECTRIC VEHICLES; LEAD-ACID-BATTERIES; STATE-OF-CHARGE; HEALTH AB The estimation of remaining useful life (RUL) of a faulty component is at the centre of system prognostics and health management. It gives operators a potent tool in decision making by quantifying how much time is left Until functionality is lost. RUL prediction needs to contend with multiple sources of errors, like modelling inconsistencies, system noise and degraded sensor fidelity, which leads to unsatisfactory performance from classical techniques like autoregressive integrated moving average (ARIMA) and extended Kalman filtering (EKF). The Bayesian theory of uncertainty management provides a way to contain these problems. The relevance vector machine (RVM), the Bayesian treatment of the well known support vector machine (SVM), a kernel-based regression/classification technique, is Used for model development. This model is incorporated into a particle filter (PF) framework, where statistical estimates of noise and anticipated operational conditions are used to provide estimates of RUL in the form of a probability density function (pdf). We present here a comparative study of the above-mentioned approaches on experimental data collected from Li-ion batteries. Batteries were chosen as an example of a complex system whose internal state variables are either inaccessible to sensors or hard to measure under operational conditions. In addition, battery performance is strongly influenced by ambient environmental and load conditions. C1 [Saha, Bhaskar; Goebel, Kai] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Saha, Bhaskar] Mission Critical Technol Inc, NASA ARC, El Segundo, CA 90245 USA. [Christophersen, Jon] Idaho Natl Lab, Idaho Falls, ID 83415 USA. RP Saha, B (reprint author), NASA, Ames Res Ctr, MS 269-3, Moffett Field, CA 94035 USA. EM bhaskar.saha_1@nasa.gov NR 17 TC 83 Z9 88 U1 6 U2 76 PU SAGE PUBLICATIONS LTD PI LONDON PA 1 OLIVERS YARD, 55 CITY ROAD, LONDON EC1Y 1SP, ENGLAND SN 0142-3312 J9 T I MEAS CONTROL JI Trans. Inst. Meas. Control PD JUN-AUG PY 2009 VL 31 IS 3-4 BP 293 EP 308 DI 10.1177/0142331208092030 PG 16 WC Automation & Control Systems; Instruments & Instrumentation SC Automation & Control Systems; Instruments & Instrumentation GA 472TD UT WOS:000268154200005 ER PT J AU Saiz-Lopez, A Adame, JA Notario, A Poblete, J Bolivar, JP Albaladejo, J AF Saiz-Lopez, A. Adame, J. A. Notario, A. Poblete, J. Bolivar, J. P. Albaladejo, J. TI Year-Round Observations of NO, NO2, O-3, SO2, and Toluene Measured with a DOAS System in the Industrial Area of Puertollano, Spain SO WATER AIR AND SOIL POLLUTION LA English DT Article DE DOAS; Air quality; Ozone; SO2; Toluene; NOx; Puertollano ID NORTHERN SPAIN; SURFACE OZONE; URBAN AREA; DEPOSITION; GREECE AB We report observations of primary and secondary atmospheric pollutants such as nitrogen oxides, sulfur dioxide, toluene, and ozone during the period February 2002 to August 2003 in Puertollano, an industrial area located in central-southern Spain. The measurements were performed using a commercial differential optical absorption spectroscopy instrument. From the hourly data, we have analyzed the mean seasonal levels and the daily evolution and we have examined the occurrence of elevated pollution episodes. The daily cycles of NO, NO2, SO2, and toluene were characterized by an early-morning maximum whereas O-3 peaks were monitored around noon. Seasonally, the highest hourly mean concentrations of NO, NO2, SO2, and toluene, 14.2, 27.0, 34.4, and 12.1 mu g m(-3) respectively, were found in the winter while O-3 summer levels reached 119.1 mu g m(-3). The dataset presented here shows episodic occurrences of elevated concentrations that exceeded the maximum levels established in the European Directives. For instance, hourly values for SO2 were repeatedly measured above 350 mu g m(-3). During the period of measurements, the O-3 thresholds (i.e., hourly value of 240 mu g m(-3)) defined to protect the human health have also been exceeded numerous times. Finally, we investigate daily and seasonal patterns in pollution levels within the context of local meteorology and photochemistry, vehicular traffic, and industrial emissions. C1 [Poblete, J.; Albaladejo, J.] Univ Castilla La Mancha, Fac Ciencias Quim, Dept Quim Fis, E-13071 Ciudad Real, Spain. [Saiz-Lopez, A.] CALTECH, Jet Prop Lab, NASA, Div Earth & Space Sci, Pasadena, CA 91109 USA. [Adame, J. A.] El Arenosillo Inst Nacl Tecn Aeroespacial INTA, Sounding Atmospher Stn, Mazagon 21130, Huelva, Spain. [Adame, J. A.; Bolivar, J. P.] Univ Huelva, Fac Ciencias Expt, Dept Fis Aplicada, Huelva, Spain. [Notario, A.] Univ Castilla La Mancha, Inst Tecnol Quim & Medioambiental ITQUIMA, E-13071 Ciudad Real, Spain. RP Albaladejo, J (reprint author), Univ Castilla La Mancha, Fac Ciencias Quim, Dept Quim Fis, Ave Camilo Jose Cela S-N, E-13071 Ciudad Real, Spain. EM Jose.Albaladejo@uclm.es RI Notario, Alberto/K-5975-2014; Saiz-Lopez, Alfonso/B-3759-2015; Albaladejo, Jose/N-3557-2014; Bolivar, Juan Pedro/F-1582-2017; Jose, Adame/K-3951-2014 OI Notario, Alberto/0000-0003-0097-6647; Saiz-Lopez, Alfonso/0000-0002-0060-1581; Albaladejo, Jose/0000-0001-8776-6807; Bolivar, Juan Pedro/0000-0001-9258-6341; Jose, Adame/0000-0002-6302-7193 FU Spanish Ministerio de Educacion y Ciencia [CGL2004-03355/CLI]; Junta de Comunidades de Castilla-La Mancha [PAI-05-062]; Junta de Andalucia [FQM2065] FX The authors gratefully thank the Spanish Ministerio de Educacion y Ciencia (Project No. CGL2004-03355/CLI), the Junta de Comunidades de Castilla-La Mancha (Project No. PAI-05-062), and the Junta de Andalucia (Project code FQM2065) for financial support of this research work. NR 20 TC 15 Z9 15 U1 0 U2 9 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0049-6979 J9 WATER AIR SOIL POLL JI Water Air Soil Pollut. PD JUN PY 2009 VL 200 IS 1-4 BP 277 EP 288 DI 10.1007/s11270-008-9912-8 PG 12 WC Environmental Sciences; Meteorology & Atmospheric Sciences; Water Resources SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences; Water Resources GA 451RN UT WOS:000266487700025 ER PT J AU Hatamleh, O Smith, J Cohen, D Bradley, R AF Hatamleh, Omar Smith, James Cohen, Donald Bradley, Robert TI Surface roughness and friction coefficient in peened friction stir welded 2195 aluminum alloy SO APPLIED SURFACE SCIENCE LA English DT Article DE Friction stir welding; Laser peening; Shot peening; Surface roughness; Friction; AA 2195 AB The tribological properties of friction stir welded 2195 aluminum alloy joints were investigated for several laser- and shot-peened specimens. The first portion of this study assessed the surface roughness changes at different regions of the weld resulting from the various peening processes and included an atomic force microscopy (AFM) study to reveal fine structures. The second portion investigated the friction characteristics for various conditions when slid against a 440C ball slider. Shot peening resulted in significant surface roughness when compared to the unpeened and laser-peened samples. The initial friction for all types of specimens was highly variable. However, long-term friction was shown to be lowest for samples with no peening treatment. Laser peening caused the friction to increase slightly. The shot peening process on the other hand resulted in an increase of the long-term friction effects on both sides of the weld. Published by Elsevier B.V. C1 [Hatamleh, Omar; Smith, James] NASA, Lyndon B Johnson Space Ctr, Struct Branch, Houston, TX 77058 USA. [Cohen, Donald] Michigan Metrol LLC, Livonia, MI 48152 USA. [Bradley, Robert] Oak Ridge Associate Univ, Houston, TX 77058 USA. RP Hatamleh, O (reprint author), NASA, Lyndon B Johnson Space Ctr, Struct Branch, Houston, TX 77058 USA. EM omar.hatamleh-1@nasa.gov NR 22 TC 13 Z9 14 U1 4 U2 17 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 MAY 30 PY 2009 VL 255 IS 16 BP 7414 EP 7426 DI 10.1016/j.apsusc.2009.04.011 PG 13 WC Chemistry, Physical; Materials Science, Coatings & Films; Physics, Applied; Physics, Condensed Matter SC Chemistry; Materials Science; Physics GA 446CI UT WOS:000266097500052 ER PT J AU Zhang, Y Fu, R Yu, HB Qian, Y Dickinson, R Dias, MAFS Dias, PLD Fernandes, K AF Zhang, Yan Fu, Rong Yu, Hongbin Qian, Yun Dickinson, Robert Silva Dias, Maria Assuncao F. da Silva Dias, Pedro L. Fernandes, Katia TI Impact of biomass burning aerosol on the monsoon circulation transition over Amazonia SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID TROPICAL SOUTH-AMERICA; LA-PLATA BASIN; MODIS RETRIEVALS; GOCART MODEL; WET SEASON; SMOKE; SATELLITE; PRECIPITATION; SIMULATIONS; ONSET AB Ensemble simulations of a regional climate model (RegCM3) forced by aerosol radiative forcing suggest that biomass burning aerosols can work against the seasonal monsoon circulation transition, thus re-enforce the dry season rainfall pattern for Southern Amazonia. Strongly absorbing smoke aerosols warm and stabilize the lower troposphere within the smoke center in southern Amazonia (where aerosol optical depth >0.3). These changes increase the surface pressure in the smoke center, weaken the southward surface pressure gradient between northern and southern Amazonia, and consequently induce an anomalous moisture divergence in the smoke center and an anomalous convergence in northwestern Amazonia (5 degrees S-5 degrees N, 60 degrees W-70 degrees W). The increased atmospheric thermodynamic stability, surface pressure, and divergent flow in Southern Amazonia may inhibit synoptic cyclonic activities propagated from extratropical South America, and re-enforce winter-like synoptic cyclonic activities and rainfall in southeastern Brazil, Paraguay and northeastern Argentina. Citation: Zhang, Y., R. Fu, H. Yu, Y. Qian, R. Dickinson, M. A. F. Silva Dias, P. L. da Silva Dias, and K. Fernandes (2009), Impact of biomass burning aerosol on the monsoon circulation transition over Amazonia, Geophys. Res. Lett., 36, L10814, doi: 10.1029/2009GL037180. C1 [Zhang, Yan; Fernandes, Katia] Georgia Inst Technol, Sch Earth & Atmospher Sci, Atlanta, GA 30332 USA. [Fu, Rong; Dickinson, Robert] Univ Texas Austin, Jackson Sch Geosci, Dept Geol Sci, Austin, TX 78705 USA. [Yu, Hongbin] Univ Maryland Baltimore Cty, Goddard Earth Sci & Technol Ctr, Baltimore, MD 21228 USA. [Yu, Hongbin] NASA, Goddard Space Flight Ctr, Atmospheres Lab, Greenbelt, MD 20771 USA. [Silva Dias, Maria Assuncao F.; da Silva Dias, Pedro L.] Univ Sao Paulo, Dept Atmospher Sci, BR-05508900 Sao Paulo, Brazil. [Qian, Yun] Pacific NW Natl Lab, Richland, WA 99352 USA. RP Zhang, Y (reprint author), Georgia Inst Technol, Sch Earth & Atmospher Sci, 311 Ferst Dr, Atlanta, GA 30332 USA. EM yan.zhang@gatech.edu RI qian, yun/A-5056-2010; Yu, Hongbin/C-6485-2008; Zhang, Yan/C-4792-2012; Silva Dias, Maria /C-5998-2012; qian, yun/E-1845-2011; Fu, Rong/B-4922-2011 OI Yu, Hongbin/0000-0003-4706-1575; FU NASA [NNG04GK90G, NNG04GB89G]; U. S. DOE [DE-AC06-76RLO1830] FX This work was supported by the NASA Aura and Atmospheric Composition Program and the Earth System Science Research using data and products from Terra, Aqua and ACRIMSAT NNG04GK90G and NNG04GB89G projects. The Pacific Northwest National Laboratory (PNNL) is operated for the U. S. DOE by Battelle Memorial Institute under contract DE-AC06-76RLO1830. NR 28 TC 28 Z9 28 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 MAY 30 PY 2009 VL 36 AR L10814 DI 10.1029/2009GL037180 PG 6 WC Geosciences, Multidisciplinary SC Geology GA 452CW UT WOS:000266518400001 ER PT J AU Signorini, SR McClain, CR AF Signorini, Sergio R. McClain, Charles R. TI Environmental factors controlling the Barents Sea spring-summer phytoplankton blooms SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID EMILIANIA-HUXLEYI; POLAR FRONT; LIGHT AB We provide an analysis of the seasonal change of the physical forcing factors and their impact on the timing and intensity of phytoplankton blooms in the Barents Sea, with emphasis on the different functional groups that can be distinguished (coccolithophores and other phytoplankton groups) using satellite remote sensing algorithms. Our analyses are based on an integration of satellite derived products and historical hydrographic data. There is a significant phase shift between the peaks of the diatom bloom in May to the coccolithophore bloom in August. Light and nutrient variability, driven by the large seasonal changes of solar irradiance and mixed layer depth in the Barents Sea, are the major environmental factors controlling these phytoplankton blooms. Based on previous field campaigns that identified Emiliana huxleyi as the most predominant species of coccolithophores in the Barents Sea, we conclude that the high concentration of calcite retrieved by ocean color satellites in summer is a result of bloom-forming coccolithophores of this species. A strong correlation between calcite concentration and wind speed squared (r(2) = 0.8) was found during the peak of the bloom. We suggest that this correlation is an indication of CO(2) fertilization resulting from regionally enhanced uptake of atmospheric CO(2). Citation: Signorini, S. R., and C. R. McClain (2009), Environmental factors controlling the Barents Sea spring-summer phytoplankton blooms, Geophys. Res. Lett., 36, L10604, doi:10.1029/2009GL037695. C1 [Signorini, Sergio R.] Sci Applicat Int Corp, Beltsville, MD 20705 USA. [McClain, Charles R.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Signorini, SR (reprint author), Sci Applicat Int Corp, 4600 Powder Mill Rd, Beltsville, MD 20705 USA. EM sergio.signorini@nasa.gov; charles.r.mcclain@nasa.gov FU NASA FX This work was funded by the NASA Ocean Biology and Biogeochemistry Program. NR 21 TC 9 Z9 9 U1 3 U2 11 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 MAY 29 PY 2009 VL 36 AR L10604 DI 10.1029/2009GL037695 PG 5 WC Geosciences, Multidisciplinary SC Geology GA 452CU UT WOS:000266518200002 ER PT J AU Yu, HB Chin, M Remer, LA Kleidman, RG Bellouin, N Bian, HS Diehl, T AF Yu, Hongbin Chin, Mian Remer, Lorraine A. Kleidman, Richard G. Bellouin, Nicolas Bian, Huisheng Diehl, Thomas TI Variability of marine aerosol fine-mode fraction and estimates of anthropogenic aerosol component over cloud-free oceans from the Moderate Resolution Imaging Spectroradiometer (MODIS) SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID OPTICAL-THICKNESS; SATELLITE; GOCART; SENSITIVITY; ATMOSPHERE; ATLANTIC; TOP AB In this study, we examine seasonal and geographical variability of marine aerosol fine-mode fraction (f(m)) and its impacts on deriving the anthropogenic component of aerosol optical depth (tau(a)) and direct radiative forcing from multispectral satellite measurements. A proxy of f(m), empirically derived from the Moderate Resolution Imaging Spectroradiometer (MODIS) Collection 5 data, shows large seasonal and geographical variations that are consistent with the Goddard Chemistry Aerosol Radiation Transport (GOCART) and Global Modeling Initiative (GMI) model simulations. The so-derived seasonally and spatially varying f(m) is then implemented into a method of estimating tau(a) and direct radiative forcing from the MODIS measurements. It is found that the use of a constant value for f(m) as in previous studies would have overestimated tau(a) by about 20% over global ocean, with the overestimation up to similar to 45% in some regions and seasons. The 7-year (2001-2007) global ocean average tau(a) is 0.035, with yearly average ranging from 0.031 to 0.039. Future improvement in measurements is needed to better separate anthropogenic aerosol from natural ones and to narrow down the wide range of aerosol direct radiative forcing. C1 [Yu, Hongbin; Chin, Mian; Remer, Lorraine A.; Kleidman, Richard G.; Bian, Huisheng; Diehl, Thomas] NASA, Goddard Space Flight Ctr, Atmospheres Lab, Greenbelt, MD 20771 USA. [Bellouin, Nicolas] Met Off, Hadley Ctr, Exeter EX1 3PB, Devon, England. [Yu, Hongbin; Bian, Huisheng; Diehl, Thomas] Univ Maryland, Goddard Earth Sci & Technol Ctr, Baltimore, MD 21201 USA. [Kleidman, Richard G.] Sci Syst & Applicat Inc, Lanham, MD USA. RP Yu, HB (reprint author), NASA, Goddard Space Flight Ctr, Atmospheres Lab, Code 613-2, Greenbelt, MD 20771 USA. EM Hongbin.Yu@nasa.gov RI Yu, Hongbin/C-6485-2008; Chin, Mian/J-8354-2012; OI Yu, Hongbin/0000-0003-4706-1575; Bellouin, Nicolas/0000-0003-2109-9559 FU UK Department for Environment, Food and Rural Affairs; Ministry of Defense Integrated Climate Programme [GA01101, CBC/2B/0417] FX The work by researchers associated with NASA was supported by NASA's Atmospheric Composition Modeling and Analysis Program, and Radiation Sciences Program. The work by N. B. was supported by the joint UK Department for Environment, Food and Rural Affairs and Ministry of Defense Integrated Climate Programme GA01101, CBC/2B/0417 Annex C5. We thank three reviewers for their helpful comments. NR 47 TC 42 Z9 43 U1 0 U2 11 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 MAY 29 PY 2009 VL 114 AR D10206 DI 10.1029/2008JD010648 PG 11 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 452DE UT WOS:000266519200003 ER PT J AU Halekas, JS Delory, GT Lin, RP Stubbs, TJ Farrell, WM AF Halekas, J. S. Delory, G. T. Lin, R. P. Stubbs, T. J. Farrell, W. M. TI Lunar surface charging during solar energetic particle events: Measurement and prediction SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article ID ADVANCED COMPOSITION EXPLORER; DYNAMIC FOUNTAIN MODEL; ACE OBSERVATIONS; WIND SPACECRAFT; DUST; ELECTRON AB We analyzed lunar surface charging during solar energetic particle (SEP) events, utilizing Lunar Prospector measurements of surface potentials and electron fluxes, and upstream energetic particle data. Outside of the magnetosphere, we find a nearly one-to-one correspondence between extreme negative lunar surface charging and large solar proton events. Using new techniques to correct for spacecraft potential, we present the first quantitative measurements of lunar charging during SEP events, during which we find that the nightside surface reaches potentials of up to -4.5 kV, with negative potentials of a kilovolt or larger often observed. These potentials are far higher than typical nightside potentials of a few hundred volts negative and may increase the risk of electrostatic discharge and/or dust effects, introducing an additional hazard to the already dangerous radiation environment. For eight of eleven event periods, surface potentials correlate with electron temperature and with the ratio of energetic electron flux to both energetic proton flux and total electron flux. For these eight events, charging models taking into account both thermal/suprathermal and energetic particle fluxes, as well as secondary emission, can successfully predict surface potentials. However, during the other three events, surface potentials do not correlate with the same measurable quantities, and charging models cannot reproduce measured potentials. In order to develop reliable and accurate models for lunar surface charging during SEP events, we will need better measurements of ion and energetic particle behavior in the lunar environment, secondary electron emission from lunar materials, and lunar surface potentials. C1 [Halekas, J. S.; Delory, G. T.; Lin, R. P.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Lin, R. P.] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA. [Stubbs, T. J.; Farrell, W. M.] NASA, Goddard Space Flight Ctr, Solar Syst Explorat Div, Greenbelt, MD 20771 USA. [Stubbs, T. J.] Univ Maryland, Goddard Earth Sci & Technol Ctr, Baltimore, MD 21201 USA. RP Halekas, JS (reprint author), Univ Calif Berkeley, Space Sci Lab, 7 Gauss Way, Berkeley, CA 94720 USA. EM jazzman@ssl.berkeley.edu RI Stubbs, Timothy/I-5139-2013; Farrell, William/I-4865-2013; OI Stubbs, Timothy/0000-0002-5524-645X; Halekas, Jasper/0000-0001-5258-6128 FU NASA [NNG06GJ23G, NNX07AG10G] FX Wolfgang Baumjohann thanks Tomoko Nakagawa and Yoshifumi Saito for their assistance in evaluating this paper. NR 40 TC 25 Z9 26 U1 1 U2 3 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0148-0227 J9 J GEOPHYS RES-SPACE JI J. Geophys. Res-Space Phys. PD MAY 28 PY 2009 VL 114 AR A05110 DI 10.1029/2009JA014113 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 452HY UT WOS:000266532200001 ER PT J AU Benson, RF Bilitza, D AF Benson, Robert F. Bilitza, Dieter TI New satellite mission with old data: Rescuing a unique data set SO RADIO SCIENCE LA English DT Article ID ELECTRON-DENSITY PROFILES; TOPSIDE SOUNDER DATA; SCALE HEIGHT; IONOSPHERE; MODEL; IONOGRAMS; PROPAGATION; IRI AB We review efforts to save a unique data set and scientific results based on the rescued data. The goal of the project was to produce Alouette 2, ISIS 1, and ISIS 2 digital topside ionograms from selected original seven-track analog telemetry tapes. This project was initiated to preserve a significant portion of 60 satellite years of analog data, collected between 1962 and 1990, in digital form before the tapes were discarded. More than 1/2 million digital topside ionograms are now available for downloading at http://nssdcftp.gsfc.nasa.gov and for browsing and plotting at http://cdaweb.gsfc.nasa.gov. We illustrate data products, discuss analysis programs, review scientific results based on the digital data, and recognize those who made the project possible. The scientific results include evidence of extremely low altitude ionospheric peak densities at high latitudes, improved and new ionospheric models including one connecting the F2 topside ionosphere and the plasmasphere, transionospheric HF propagation investigations, and new interpretations of sounder-stimulated plasma emissions that have challenged theorists for decades. The homepage for the ISIS project is at http://nssdc.gsfc.nasa.gov/space/isis/isis-status.html. C1 [Benson, Robert F.] NASA, Goddard Space Flight Ctr, Geospace Phys Lab, Greenbelt, MD 20771 USA. [Bilitza, Dieter] NASA, Goddard Space Flight Ctr, Heliophys Lab, Greenbelt, MD 20771 USA. [Bilitza, Dieter] George Mason Univ, Space Weather Lab, Fairfax, VA 22030 USA. RP Benson, RF (reprint author), NASA, Goddard Space Flight Ctr, Geospace Phys Lab, Greenbelt, MD 20771 USA. EM dieter.bilitza.1@gsfc.nasa.gov FU NASA LWS TRT award; NASA GSFC FX Our first tribute to those who make this work possible goes to H. Gordon James who sounded the alarm when the data set was in danger of being permanently lost. He assisted the authors in the selection of the tapes to be processed, arranged for their shipment from Canada to the NASA GSFC, and provided valuable supporting information about the ISIS topside sounders. NASA's ITM Data Evaluation Panel helped the cause by giving the ISIS data restoration effort highest priority. Funding was first provided by the late Jim Willett, following the advice of his data panel, continued with the enthusiastic support of Joe Bredekamp, via the NASA AISR program, and later under a NASA LWS TR&T award, and internal NASA GSFC support with the assistance of Jim Slavin and Ed Grayzek. The design and setup of the A/D process was primarily the effort of Frank Ross, the late John Limpert, the late Joe Iffrig, Jerry Larner, Clyde Freeman (who, as the former ISIS Data Processing Engineer, also provided important guidance throughout the project), Les Johnson, and Jim Hill. The creation of the digital topside ionograms is the result of the programming skills of the late John Limpert and the late Bill Schar who also provided quality control and helped train the A/D operators Mary King, Dawn Canty, and Hal Harris. The bulk of the routine A/ D transformation of the original analog telemetry tapes to produce the digital topside ionograms has been the result of the skilled effort of Mary King with the gifted technical assistance of Dick Bouchard to keep the Bell and Howell tape recorders, Monitor Bit and Frame Syncs, Datatron Time-Code Translator, and IBM 486 pc ( running OS2-WARP) operational based on his decades of experience. His technical experience complemented the assistance provided by Sarma Velamuri and Daniel Emery who made necessary software modifications to overcome problems encountered. Dick Brown provided management support. At the NSSDC, under the guidance of Joe King, the data pipeline (including conversion to CDF for display on CDAWeb and archiving on nssdcftp) was set up by Rich Baldwin with help from Karen Horrocks, and Howard Leckner. Day-to-day operations were maintained by Ralph Post, Barbara Rowland, Nelson Cheung, and Celest Lindsay. Len Moriarty and former summer intern Suzan Dent, working with Bill Schar, designed a web interface for searching the database for user- specified conditions. Gary Burgess developed the NSSDC program for the analysis of digital topside ionograms, based on the inversion routine of John E. Jackson, and also assisted with the ionogram quality control. Xueqin Huang created the TOPIST software, under the guidance of Bodo Reinisch, and H. Kent Hills applied it to ISIS 2 digital topside ionograms to produce topside Ne(h) profiles. A variety of funding sources have made the preservation and (A/D) transformation of the Alouette and ISIS topside sounder data possible as summarized in section 1. We are grateful to valuable comments and suggestions from three reviewers and to P. A. Webb for the production of Figure NR 39 TC 9 Z9 9 U1 1 U2 2 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 MAY 28 PY 2009 VL 44 AR RS0A04 DI 10.1029/2008RS004036 PG 14 WC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology & Atmospheric Sciences; Remote Sensing; Telecommunications SC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology & Atmospheric Sciences; Remote Sensing; Telecommunications GA 452ML UT WOS:000266544200001 ER PT J AU Sakaki, K Date, R Mizuno, M Araki, H Nakamura, Y Shirai, Y Bowman, RC Akiba, E AF Sakaki, Kouji Date, Ryosuke Mizuno, Masataka Araki, Hideki Nakamura, Yumiko Shirai, Yasuharu Bowman, Robert C., Jr. Akiba, Etsuo TI Behavior of vacancy formation and recovery during hydrogenation cycles in LaNi(4.93)Sn(0.27) SO JOURNAL OF ALLOYS AND COMPOUNDS LA English DT Article DE Positron annihilation; Hydrogen storage; Vacancy; Dislocation ID POSITRON LIFETIME SPECTRA; X-RAY-DIFFRACTION; INITIAL ACTIVATION PROCESS; LATTICE-DEFECTS; LANI5; SYSTEM; ANNIHILATION; PROGRAM; STRAIN; DEGRADATION AB To clarify the effect of substitution of Sn for Ni of LaNi(5) on cyclic durability of hydrogen storage, the behavior of lattice defects during the hydrogenation cycles at 288 K in LaNi(4.93)Sn(0.27) was investigated by in situ positron lifetime measurements. Mean positron lifetime increased to 175 ps by vacancy formation during initial hydrogenation and then decreased to 135 ps by vacancy recovery during dehydrogenation. Vacancies were reversibly introduced and removed at 288 K, although quenched-in vacancy cannot migrate below 448 K in LaNi(4.93)Sn(0.27). Reversible change of the positron lifetime was observed in subsequent cycles, and dislocation density and vacancy concentration remained almost constant at around 6 x 10(9) cm(-2) and 10 ppm, respectively, which are two orders of magnitude lower than those in binary LaNi(5). These results indicate that the degradation of hydrogen capacity during a cycle closely relates to the concentration of lattice defects accumulated with hydrogenation. (C) 2008 Elsevier B.V. All rights reserved. C1 [Sakaki, Kouji; Nakamura, Yumiko; Akiba, Etsuo] Natl Inst Adv Ind Sci & Technol, Tsukuba, Ibaraki 3058565, Japan. [Date, Ryosuke; Mizuno, Masataka; Araki, Hideki; Shirai, Yasuharu] Osaka Univ, Dept Mat Sci & Engn, Osaka 5650871, Japan. [Bowman, Robert C., Jr.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Sakaki, K (reprint author), Natl Inst Adv Ind Sci & Technol, 1-1-1 Higashi, Tsukuba, Ibaraki 3058565, Japan. EM kouji.sakaki@aist.go.jp FU New Energy and Industrial Technology Development Organization (NEDO); Ministry of Economy, Trade, and Industry (METI) of Japan FX A part of this work has been supported by New Energy and Industrial Technology Development Organization (NEDO) under its "Advanced Fundamental Research Project on Hydrogen Storage Materials." A part of this research was also financially supported by the Ministry of Economy, Trade, and Industry (METI) of Japan. This research was partially performed at the jet Propulsion Laboratory, which is operated by the California Institute of Technology under contract with the U.S. National Aeronautics and Space Administration (NASA). NR 32 TC 9 Z9 9 U1 0 U2 8 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 MAY 27 PY 2009 VL 477 IS 1-2 BP 205 EP 211 DI 10.1016/j.jallcom.2008.10.058 PG 7 WC Chemistry, Physical; Materials Science, Multidisciplinary; Metallurgy & Metallurgical Engineering SC Chemistry; Materials Science; Metallurgy & Metallurgical Engineering GA 450FM UT WOS:000266386400048 ER PT J AU Robock, A Ammann, CM Oman, L Shindell, D Levis, S Stenchikov, G AF Robock, Alan Ammann, Caspar M. Oman, Luke Shindell, Drew Levis, Samuel Stenchikov, Georgiy TI Did the Toba volcanic eruption of similar to 74 ka BP produce widespread glaciation? SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID CLIMATE SYSTEM MODEL; SUPER-ERUPTION; VERSION-3 CCSM3; SIMULATIONS; IMPACT; CONSEQUENCES; BOTTLENECK; ATMOSPHERE; WINTER; OCEAN AB It has been suggested that the Toba volcanic eruption, approximately 74 ka B. P., was responsible for the extended cooling period and ice sheet advance immediately following it, but previous climate model simulations, using 100 times the amount of aerosols produced by the 1991 Mount Pinatubo eruption, have been unable to produce such a prolonged climate response. Here we conduct six additional climate model simulations with two different climate models, the National Center for Atmospheric Research Community Climate System Model 3.0 (CCSM3.0) and National Aeronautics and Space Administration Goddard Institute for Space Studies ModelE, in two different versions, to investigate additional mechanisms that may have enhanced and extended the forcing and response from such a large supervolcanic eruption. With CCSM3.0 we include a dynamic vegetation model to explicitly calculate the feedback of vegetation death on surface fluxes in response to the large initial reduction in transmitted light, precipitation, and temperature. With ModelE we explicitly calculate the effects of an eruption on stratospheric water vapor and model stratospheric chemistry feedbacks that might delay the conversion of SO2 into sulfate aerosols and prolong the lifetime and radiative forcing of the stratospheric aerosol cloud. To span the uncertainty in the amount of stratospheric injection of SO2, with CCSM3.0 we used 100 times the Pinatubo injection, and with ModelE we used 33, 100, 300, and 900 times the Pinatubo injection without interactive chemistry, and 300 times Pinatubo with interactive chemistry. Starting from a roughly present-day seasonal cycle of insolation, CO2 concentration, and vegetation, or with 6 ka B. P. conditions for CCSM3.0, none of the runs initiates glaciation. The CCSM3.0 run produced a maximum global cooling of 10 K and ModelE runs produced 8-17 K of cooling within the first years of the simulation, depending on the injection, but in all cases, the climate recovers over a few decades. Nevertheless, the "volcanic winter'' following a supervolcano eruption of the size of Toba today would have devastating consequences for humanity and global ecosystems. These simulations support the theory that the Toba eruption indeed may have contributed to a genetic bottleneck. C1 [Robock, Alan; Stenchikov, Georgiy] Rutgers State Univ, Dept Environm Sci, Brunswick, NJ 08901 USA. [Ammann, Caspar M.; Levis, Samuel] Natl Ctr Atmospher Res, Boulder, CO 80307 USA. [Oman, Luke] Johns Hopkins Univ, Dept Earth & Planetary Sci, Baltimore, MD 21218 USA. [Shindell, Drew] NASA, Goddard Inst Space Studies, New York, NY 10025 USA. RP Robock, A (reprint author), Rutgers State Univ, Dept Environm Sci, 14 Coll Farm Rd, Brunswick, NJ 08901 USA. EM robock@envsci.rutgers.edu; ammann@ucar.edu; oman@jhu.edu; dshindell@giss.nasa.gov; slevis@ucar.edu; gera@envsci.rutgers.edu RI Oman, Luke/C-2778-2009; Shindell, Drew/D-4636-2012; Georgiy, Stenchikov/J-8569-2013; Robock, Alan/B-6385-2016 OI Oman, Luke/0000-0002-5487-2598; FU NASA [NNG05GB06G]; NSF [ATM-0313592, ATM-0351280, ATM-0730452] FX We thank two anonymous reviewers and Stephen Self for valuable suggestions, and we thank Greg Faluvegi for scientific programming support at GISS. This work is supported by NASA grant NNG05GB06G and NSF grants ATM-0313592, ATM-0351280, and ATM-0730452. Model development and computer time at GISS are supported by NASA climate modeling and atmospheric chemistry modeling grants. The National Center for Atmospheric Research is supported by the National Science Foundation. NR 39 TC 57 Z9 59 U1 33 U2 81 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 MAY 27 PY 2009 VL 114 AR D10107 DI 10.1029/2008JD011652 PG 9 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 452DD UT WOS:000266519100004 ER PT J AU Glocer, A Toth, G Gombosi, T Welling, D AF Glocer, A. Toth, G. Gombosi, T. Welling, D. TI Modeling ionospheric outflows and their impact on the magnetosphere, initial results SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article ID POLAR WIND; ION COMPOSITION; THERMOSPHERIC MODEL; RING CURRENT; MAGNETOHYDRODYNAMICS; DYNAMICS; CURRENTS; SPACE; STORM AB Ionospheric outflow has been shown to be a significant contributor to the plasma population of the magnetosphere during active geomagnetic conditions. We present the results of new efforts to model the source and effects of out-flowing plasma in the Space Weather Modeling Framework (SWMF). In particular, we develop and use the Polar Wind Outflow Model (PWOM), a field-aligned, multifluid, multifield line polar wind code to simulate the ionospheric outflow. The PWOM is coupled to the ionosphere electrodynamics and global magnetosphere components of the SWMF, so we can calculate the outflow and its resulting impact on magnetospheric composition and dynamics. By including the outflow as part of a coupled system, we study the consequences of outflow on the larger space environment system. We present our methodology for the magnetosphere-ionosphere coupling, as well as the effect of outflow on the magnetosphere during two geomagnetic storms. Moreover, we explore the use of multispecies MHD to track the resulting plasma composition in the magnetosphere. We find that, by including ionospheric outflow during geomagnetic storms, we can reduce the RMS error in the simulated magnetic field as compared with various GOES satellites by as much as 50%. Additionally, we find that the outflow causes a strong decrease in Dst and in the cross-polar cap potential. C1 [Glocer, A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Toth, G.; Gombosi, T.; Welling, D.] Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA. RP Glocer, A (reprint author), NASA, Goddard Space Flight Ctr, Code 673, Greenbelt, MD 20771 USA. EM alex.glocer-1@nasa.gov RI Gombosi, Tamas/G-4238-2011; Glocer, Alex/C-9512-2012; Toth, Gabor/B-7977-2013; Welling, Daniel/C-1970-2013; feggans, john/F-5370-2012 OI Gombosi, Tamas/0000-0001-9360-4951; Glocer, Alex/0000-0001-9843-9094; Toth, Gabor/0000-0002-5654-9823; NR 47 TC 59 Z9 59 U1 0 U2 8 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9380 J9 J GEOPHYS RES-SPACE JI J. Geophys. Res-Space Phys. PD MAY 27 PY 2009 VL 114 AR A05216 DI 10.1029/2009JA014053 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 452HU UT WOS:000266531800002 ER PT J AU Smelyanskiy, VN Luchinsky, DG Millonas, MM McClintock, PVE AF Smelyanskiy, V. N. Luchinsky, D. G. Millonas, M. M. McClintock, P. V. E. TI Recovering 'lost' information in the presence of noise: application to rodent-predator dynamics SO NEW JOURNAL OF PHYSICS LA English DT Article ID MODELS; CHAOS; SYSTEMS; CYCLES AB A Hamiltonian approach is introduced for the reconstruction of trajectories and models of complex stochastic dynamics from noisy measurements. The method converges even when entire trajectory components are unobservable and the parameters are unknown. It is applied to reconstruct nonlinear models of rodent-predator oscillations in Finnish Lapland and high-Arctic tundra. The projected character of noisy incomplete measurements is revealed and shown to result in a degeneracy of the likelihood function within certain null-spaces. The performance of the method is compared with that of the conventional Markov chain Monte Carlo (MCMC) technique. C1 [Smelyanskiy, V. N.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Luchinsky, D. G.] Mission Crit Technol Inc, El Segundo, CA 90245 USA. [Luchinsky, D. G.; McClintock, P. V. E.] Univ Lancaster, Dept Phys, Lancaster LA1 4YB, England. [Millonas, M. M.] CardioPrint Biometr Inc, Boulder Creek, CA 95006 USA. RP Smelyanskiy, VN (reprint author), NASA, Ames Res Ctr, MS 269-2, Moffett Field, CA 94035 USA. EM Vadim.N.Smelyanskiy@nasa.gov; d.luchinsky@lancaster.ac.uk; millonas@cardioprint.com; p.v.e.mcclintock@lancaster.ac.uk RI Luchinsky, Dmitry/N-4177-2014 FU NASA; Engineering and Physical Sciences Research Council (UK) FX We acknowledge support from NASA and the Engineering and Physical Sciences Research Council (UK). NR 25 TC 1 Z9 1 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 1367-2630 J9 NEW J PHYS JI New J. Phys. PD MAY 27 PY 2009 VL 11 AR 053012 DI 10.1088/1367-2630/11/5/053012 PG 10 WC Physics, Multidisciplinary SC Physics GA 451GJ UT WOS:000266458400001 ER PT J AU Veca, LM Meziani, MJ Wang, W Wang, X Lu, FS Zhang, PY Lin, Y Fee, R Connell, JW Sun, YP AF Veca, L. Monica Meziani, Mohommed J. Wang, Wei Wang, Xin Lu, Fushen Zhang, Puyu Lin, Yi Fee, Robert Connell, John W. Sun, Ya-Ping TI Carbon Nanosheets for Polymeric Nanocomposites with High Thermal Conductivity SO ADVANCED MATERIALS LA English DT Article ID NANOTUBE COMPOSITES; GRAPHENE; FILMS; ENHANCEMENT; MANAGEMENT; BLENDS AB Nanometer-thick 2D carbon structures ("carbon nanosheets") are processed from commercially available expanded graphite. These carbon nanosheets are then incorporated in various polymers to produce flexible nanocomposites that exhibit record-setting anisotropic thermal conductivities, which may prove highly valuable in many technological applications. C1 [Veca, L. Monica; Meziani, Mohommed J.; Wang, Wei; Wang, Xin; Lu, Fushen; Zhang, Puyu; Lin, Yi; Fee, Robert; Sun, Ya-Ping] Clemson Univ, Dept Chem, Clemson, SC 29634 USA. [Veca, L. Monica; Meziani, Mohommed J.; Wang, Wei; Wang, Xin; Lu, Fushen; Zhang, Puyu; Lin, Yi; Fee, Robert; Sun, Ya-Ping] Clemson Univ, Lab Emerging Mat & Technol, Clemson, SC 29634 USA. [Connell, John W.] NASA, Langley Res Ctr, Adv Mat & Proc Branch, Hampton, VA 23681 USA. RP Sun, YP (reprint author), Clemson Univ, Dept Chem, Clemson, SC 29634 USA. EM syaping@CLEMSON.edu RI Veca, Lucia/A-4622-2012; OI Lu, Fushen/0000-0002-3323-7181 FU Carolina Space Grant Consortium; NASA; NSF; Center for Advanced Engineering Fibers and Films FX Financial support from the South Carolina Space Grant Consortium, NASA, NSF, and the Center for Advanced Engineering Fibers and Films (NSF-ERC at Clemson University) is gratefully acknowledged. R.F. was a participant of the undergraduate research program jointly sponsored by NSF and Clemson University. NR 33 TC 166 Z9 174 U1 19 U2 186 PU WILEY-V C H VERLAG GMBH PI WEINHEIM PA POSTFACH 101161, 69451 WEINHEIM, GERMANY SN 0935-9648 EI 1521-4095 J9 ADV MATER JI Adv. Mater. PD MAY 25 PY 2009 VL 21 IS 20 BP 2088 EP 2092 DI 10.1002/adma.200802317 PG 5 WC Chemistry, Multidisciplinary; Chemistry, Physical; Nanoscience & Nanotechnology; Materials Science, Multidisciplinary; Physics, Applied; Physics, Condensed Matter SC Chemistry; Science & Technology - Other Topics; Materials Science; Physics GA 452HW UT WOS:000266532000015 ER PT J AU Ray, AK Whittenberger, JD AF Ray, A. K. Whittenberger, J. D. TI Stress rupture behavior of a thermal barrier coated AE 437A Ni-based superalloy used for aero turbine blades SO MATERIALS SCIENCE AND ENGINEERING A-STRUCTURAL MATERIALS PROPERTIES MICROSTRUCTURE AND PROCESSING LA English DT Article DE Thermal barrier coating; Superalloy; Bond coat; Stress rupture; Rupture life ID ACOUSTIC-EMISSION; BOND COAT; MECHANICAL-PROPERTIES; EB-PVD; FATIGUE; ENGINES; PERFORMANCE; RESISTANCE; ALUMINUM; ALLOYS AB The stress rupture characteristics of bare and thermal barrier coated (TBC) superalloy AE 437A were determined in air at temperatures between 600 and 850 degrees C with both short and long term testing undertaken at 800 degrees C. Because the bond coat contributed an addition similar to 10% cross-sectional area and was able to support load, the higher stress, shorter term rupture lives of the TBC coated alloy exceed those for the bare material. However under lower stress, longer life conditions the ability of the bond coat to support loading was reduced, and the rupture lives of both bare and TBC coated alloy were similar. (C) 2009 Elsevier B.V. All rights reserved. C1 [Ray, A. K.] CSIR, Natl Met Lab, Div Mat Sci & Technol, Jamshedpur 831007, Bihar, India. [Whittenberger, J. D.] NASA, Lewis Res Ctr, Cleveland, OH 44135 USA. RP Ray, AK (reprint author), CSIR, Natl Met Lab, Div Mat Sci & Technol, PO Burmamines, Jamshedpur 831007, Bihar, India. EM ray.ashok@rediffmail.com RI Sahu, Anjani/E-7590-2015 NR 37 TC 6 Z9 7 U1 2 U2 11 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 MAY 25 PY 2009 VL 509 IS 1-2 BP 111 EP 114 DI 10.1016/j.msea.2009.01.033 PG 4 WC Nanoscience & Nanotechnology; Materials Science, Multidisciplinary; Metallurgy & Metallurgical Engineering SC Science & Technology - Other Topics; Materials Science; Metallurgy & Metallurgical Engineering GA 444QO UT WOS:000265995700017 ER PT J AU Altobelli, N Spilker, L Pilorz, S Leyrat, C Eddgington, S Wallis, B Flandes, A AF Altobelli, N. Spilker, L. Pilorz, S. Leyrat, C. Eddgington, S. Wallis, B. Flandes, A. TI Thermal phase curves observed in Saturn's main rings by Cassini-CIRS: Detection of an opposition effect? SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID ASTEROIDS; DEPENDENCE; SPECTRA; PHYSICS; SYSTEM; MODEL AB We report on thermal phase curve measurements of Saturn's main rings by the CIRS infrared spectrometer on-board the CASSINI spacecraft. The extensive data set acquired by Cassini since its insertion in orbit around Saturn provides for the first time spatially resolved temperature measurements over broad phase angle ranges and for different solar elevations. Each of these curves exhibit a nonlinear variation in temperature with phase angle, with pronounced surges at medium to low phase angles that we interpret as an opposition effect in thermal infrared. The transition from a relatively flat linear regime to an exponential behavior in the A and B rings occurs at phase angles of 30 degrees to 40 degrees and is significantly broader in the C ring and Cassini Division. Analytical description of the phase curves is provided to serve as basis for future modeling work. The role played by mutual shadowing as possible origin of the broad thermal surge in thicker ring regions is emphasized. In turn, regolith properties might be inferred from the thermal phase curves in the optically thin ring regions. Citation: Altobelli, N., L. Spilker, S. Pilorz, C. Leyrat, S. Eddgington, B. Wallis, and A. Flandes (2009), Thermal phase curves observed in Saturn's main rings by Cassini-CIRS: Detection of an opposition effect?, Geophys. Res. Lett., 36, L10105, doi:10.1029/2009GL038163. C1 [Altobelli, N.] ESA, ESAC, E-28080 Madrid, Spain. [Spilker, L.; Pilorz, S.; Leyrat, C.; Eddgington, S.; Wallis, B.; Flandes, A.] NASA JPL, Pasadena, CA 91109 USA. RP Altobelli, N (reprint author), ESA, ESAC, POB 50727, E-28080 Madrid, Spain. EM nicolas.altobelli@sciops.esa.int NR 22 TC 11 Z9 11 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 MAY 23 PY 2009 VL 36 AR L10105 DI 10.1029/2009GL038163 PG 5 WC Geosciences, Multidisciplinary SC Geology GA 449XE UT WOS:000266363300006 ER PT J AU Liu, HY Crawford, JH Considine, DB Platnick, S Norris, PM Duncan, BN Pierce, RB Chen, G Yantosca, RM AF Liu, Hongyu Crawford, James H. Considine, David B. Platnick, Steven Norris, Peter M. Duncan, Bryan N. Pierce, Robert B. Chen, Gao Yantosca, Robert M. TI Sensitivity of photolysis frequencies and key tropospheric oxidants in a global model to cloud vertical distributions and optical properties SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID COMMUNITY CLIMATE MODEL; SOLAR-RADIATION; SEASONAL-VARIATIONS; EARTHS ATMOSPHERE; RATE COEFFICIENTS; TRACE-P; OZONE; PHOTODISSOCIATION; CHEMISTRY; SYSTEM AB Clouds directly affect tropospheric photochemistry through modification of solar radiation that determines photolysis frequencies. As a follow-up study to our recent assessment of these direct radiative effects of clouds on tropospheric chemistry, this paper presents an analysis of the sensitivity of such effects to cloud vertical distributions and optical properties (cloud optical depths (CODs) and cloud single scattering albedo), in a global three-dimensional (3-D) chemical transport model. The model was driven with a series of meteorological archives (GEOS-1 in support of the Stratospheric Tracers of Atmospheric Transport mission, or GEOS1-STRAT, GEOS-3, and GEOS-4) generated by the NASA Goddard Earth Observing System (GEOS) data assimilation system. Clouds in GEOS1-STRAT and GEOS-3 have more similar vertical distributions (with substantially smaller CODs in GEOS1-STRAT) while those in GEOS-4 are optically much thinner in the tropical upper troposphere. We find that the radiative impact of clouds on global photolysis frequencies and hydroxyl radical (OH) is more sensitive to the vertical distribution of clouds than to the magnitude of column CODs. With random vertical overlap for clouds, the model calculated changes in global mean OH (J((OD)-D-1), J(NO2)) due to the radiative effects of clouds in June are about 0.0% (0.4%, 0.9%), 0.8% (1.7%, 3.1%), and 7.3% (4.1%, 6.0%) for GEOS1-STRAT, GEOS-3, and GEOS-4, respectively; the geographic distributions of these quantities show much larger changes, with maximum decrease in OH concentrations of similar to 15-35% near the midlatitude surface. The much larger global impact of clouds in GEOS-4 reflects the fact that more solar radiation is able to penetrate through the optically thin upper tropospheric clouds, increasing backscattering from low-level clouds. Model simulations with each of the three cloud distributions all show that the change in the global burden of ozone due to clouds is less than 5%. Model perturbation experiments with GEOS-3, where the magnitude of 3-D CODs are progressively varied from -100% to 100%, predict only modest changes (<5%) in global mean OH concentrations. J((OD)-D-1), J(NO2), and OH concentrations show the strongest sensitivity for small CODs and become insensitive at large CODs owing to saturation effects. Caution should be exercised not to use in photochemical models a value for cloud single scattering albedo lower than about 0.999 in order to be consistent with the current knowledge of cloud absorption at the ultraviolet wavelengths. C1 [Liu, Hongyu; Crawford, James H.; Considine, David B.; Pierce, Robert B.; Chen, Gao] NASA, Langley Res Ctr, Chem & Dynam Branch, Hampton, VA 23681 USA. [Duncan, Bryan N.] NASA, Goddard Space Flight Ctr, Atmospher Chem & Dynam Branch, Greenbelt, MD 20771 USA. [Norris, Peter M.] NASA, Goddard Space Flight Ctr, Global Modeling & Assimilat Off, Greenbelt, MD 20771 USA. [Platnick, Steven] NASA, Goddard Space Flight Ctr, Climate & Radiat Branch, Greenbelt, MD 20771 USA. [Yantosca, Robert M.] Harvard Univ, Div Engn & Appl Sci, Cambridge, MA 02138 USA. [Liu, Hongyu] Natl Inst Aerosp, Hampton, VA USA. [Norris, Peter M.] Univ Maryland, Goddard Earth Sci & Technol Ctr, Baltimore, MD 21201 USA. RP Liu, HY (reprint author), NASA, Langley Res Ctr, Chem & Dynam Branch, Mail Stop 401B, Hampton, VA 23681 USA. EM hyl@nianet.org; james.h.crawford@nasa.gov; david.b.considine@nasa.gov; steven.platnick@nasa.gov; peter.m.norris@nasa.gov; bryan.n.duncan@nasa.gov; brad.pierce@noaa.gov; gao.chen@nasa.gov; yantosca@seas.harvard.ed RI Liu, Hongyu/A-5867-2008; Pierce, Robert Bradley/F-5609-2010; Duncan, Bryan/A-5962-2011; Norris, Peter/H-2008-2012; Crawford, James/L-6632-2013; Yantosca, Robert/F-7920-2014; Platnick, Steven/J-9982-2014 OI Pierce, Robert Bradley/0000-0002-2767-1643; Norris, Peter/0000-0001-6807-9884; Crawford, James/0000-0002-6982-0934; Yantosca, Robert/0000-0003-3781-1870; Platnick, Steven/0000-0003-3964-3567 FU NASA Langley Research Center FX This work was supported by NASA Langley Research Center. Thanks are owed to Jennifer Logan (Harvard University) for discussions that inspired part of this work, Bernhard Mayer (Institute of Atmospheric Physics of DLR, Germany) for discussions regarding the cloud single scattering albedo, Yan Feng (University of California at San Diego) for communications about the effect of cloud overlap on photolysis frequencies, and Mat Evans (University of Leeds, UK) for his comments on an earlier manuscript. MODIS and ISCCP products are distributed by NASA Goddard Level 1 and Atmosphere Archive and Distribution System http://ladsweb.nascom.nasa.gov) and Langley Atmospheric Sciences Data Center, respectively. The GEOS-Chem model is managed by the Atmospheric Chemistry Modeling Group at Harvard University with support from the NASA Atmospheric Chemistry Modeling and Analysis Program (ACMAP). The views, opinions, and findings contained in this report are those of the authors and should not be construed as an official NASA, NOAA, or U. S. government position, policy, or decision. NR 44 TC 3 Z9 4 U1 0 U2 10 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X EI 2169-8996 J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD MAY 23 PY 2009 VL 114 AR D10305 DI 10.1029/2008JD011503 PG 17 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 449XL UT WOS:000266364000006 ER PT J AU Mach, DM Blakeslee, RJ Bateman, MG Bailey, JC AF Mach, Douglas M. Blakeslee, Richard J. Bateman, Monte G. Bailey, Jeffrey C. TI Electric fields, conductivity, and estimated currents from aircraft overflights of electrified clouds SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID THUNDERSTORMS; RADAR; STEPS; SYSTEMS; STORM; CONVECTION; PLATFORMS; MICROWAVE; AIRBORNE; CIRCUIT AB Using rotating vane electric field mills and Gerdien capacitors, we measured the electric field profile and conductivity during 850 overflights of clouds and thunderstorms. The measurements were made with NASA ER-2 and Altus-II aircrafts. Peak electric fields, with lightning transients removed, ranged from -1.0 kV m(-1) to 16. kV m(-1), with a mean value of 0.9 kV m(-1). The median peak field was 0.29 kV m(-1). Flash rates ranged from 0 to over 27 flashes min(-1) with the mean flash rate of 1.2 flashes min(-1). The median flash rate for an overpass was 0.25 flashes min(-1). The positive plus negative conductivity ranged from 0.6 pS m(-1) to 3.6 pS m(-1) at the nominal flight altitudes of 15 to 20 km. The mean and median total conductivity was 2.2 pS m(-1). Peak current densities during the overpasses ranged from -2.0 nA m(-2) to 33. nA m(-2). The mean peak current density was 1.9 nA m(-2), and the median value was 0.6 nA m(-2). Using the peak electric fields, a median field falloff with distance based on all overflights, and cylindrical storm symmetry, the total upward current flow from storms in our data set ranges from -1.3 to 9.4 A with a mean value of 0.8 A. The median total current was 0.27 A. The contributions from lightning field changes do not significantly affect the total derived currents. We found that 7% of the storms were producing current flows above the storms that were opposite in polarity from the standard role that thunderstorms play in the global electric circuit. Approximately one third of the storms had no detectable lightning during the overpasses but still had significant electric fields. Owing to a possible sampling bias, the fraction of nonlightning storms with electric fields may not reflect the global probability of these clouds. C1 [Mach, Douglas M.; Bailey, Jeffrey C.] Univ Alabama, Ctr Earth Syst Sci, Huntsville, AL 35805 USA. [Bateman, Monte G.] Univ Space Res Assoc, Huntsville, AL 35805 USA. [Blakeslee, Richard J.] NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35805 USA. RP Mach, DM (reprint author), Univ Alabama, Ctr Earth Syst Sci, Huntsville, AL 35805 USA. EM doug.mach@msfc.nasa.gov FU NASA's Earth Science Enterprise (ESE); Altus; NASA's Research and Technology Operating Plan (RTOP); Research Opportunities in Space and Earth Science (ROSES); Earth Observing System (EOS); Uninhabited Aerial Vehicle Science Demonstration Project (UAV SDP) FX The authors gratefully thank NASA's Earth Science Enterprise (ESE) and program managers Ramesh Kakar (ER-2, general data analysis) and Cheryl Yuhas (Altus) for support of this research. The aircraft data used in this study were acquired during flight campaigns supported by NASA's Research and Technology Operating Plan (RTOP) and Research Opportunities in Space and Earth Science (ROSES) awards, Earth Observing System (EOS) support (for general data analysis), and the Uninhabited Aerial Vehicle Science Demonstration Project (UAV SDP). We would like to thank Charles Croskey for providing the conductivity data from the ACES project and Gerry Heymsfield for providing the EDOP radar data. The authors would also like to thank Earle Williams for his many helpful comments and suggestions made during the preparation of this paper along with the comments and suggestions from two anonymous reviewers. NR 41 TC 25 Z9 26 U1 0 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 MAY 23 PY 2009 VL 114 AR D10204 DI 10.1029/2008JD011495 PG 15 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 449XL UT WOS:000266364000005 ER PT J AU Pierce, RB Al-Saadi, J Kittaka, C Schaack, T Lenzen, A Bowman, K Szykman, J Soja, A Ryerson, T Thompson, AM Bhartia, P Morris, GA AF Pierce, R. Bradley Al-Saadi, Jassim Kittaka, Chieko Schaack, Todd Lenzen, Allen Bowman, Kevin Szykman, Jim Soja, Amber Ryerson, Tom Thompson, Anne M. Bhartia, Pawan Morris, Gary A. TI Impacts of background ozone production on Houston and Dallas, Texas, air quality during the Second Texas Air Quality Study field mission SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID TROPOSPHERIC OZONE; MONITORING INSTRUMENT; AURA MISSION; OBJECTIVES; RETRIEVAL; MECHANISM; EMISSIONS; SYSTEM; ASIA; TES AB A major objective of the 2006 Second Texas Air Quality Study (TexAQS II) focused on understanding the effects of regional processes on Houston and Dallas ozone nonattainment areas. Here we quantify the contributions of background (continental scale) ozone production on Houston and Dallas air quality during TexAQS II using ensemble Lagrangian trajectories to identify remote source regions that impact Houston and Dallas background ozone distributions. Global-scale chemical analyses, constrained with composition measurements from instruments on the NASA Aura satellite, are used to provide estimates of background composition along ensemble back trajectories. Lagrangian averaged O-3 net photochemical production (production minus loss, P-L) rates along the back trajectories are used as a metric to classify back trajectories. Results show that the majority (6 out of 9 or 66%) of the periods of high ozone in Houston were associated with periods of enhanced background ozone production. Slightly less than 50% (7 out of 15) of the days with high ozone in the Dallas Metropolitan Statistical Area (MSA) show enhanced background ozone production. Source apportionment studies show that 5-day Lagrangian averaged O-3 P-L in excess of 15 ppbv/d can occur during continental-scale transport to Houston owing to NOy enhancements from emissions within the Southern Great Lakes as well as recirculation of the Houston emissions. Dallas background O-3 P-L is associated with NOy enhancements from emissions within Chicago and Houston. C1 [Pierce, R. Bradley] NOAA, NESDIS, Adv Satellite Prod Branch, Ctr Satellite Applicat & Res,Cooperat Res Program, Madison, WI 53706 USA. [Al-Saadi, Jassim] NASA, Langley Res Ctr, Chem & Dynam Branch, Sci Directorate, Hampton, VA 23681 USA. [Bhartia, Pawan] NASA, Goddard Space Flight Ctr, Atmospheres Lab, Code 613, Greenbelt, MD 20771 USA. [Bowman, Kevin] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Kittaka, Chieko] Sci Syst & Applicat Inc, Hampton, VA 23666 USA. [Schaack, Todd; Lenzen, Allen] Univ Wisconsin, Ctr Space Sci & Engn, Madison, WI 53706 USA. [Morris, Gary A.] Valparaiso Univ, Dept Phys & Astron, Valparaiso, IN 46383 USA. [Ryerson, Tom] NOAA, Earth Syst Res Lab, Div Chem Sci, Boulder, CO 80305 USA. [Soja, Amber] Natl Inst Aerosp, Hampton, VA 23666 USA. [Thompson, Anne M.] Penn State Univ, Dept Meteorol, University Pk, PA 16802 USA. [Szykman, Jim] NASA, Langley Res Ctr, Natl Exposure Res Lab, Off Res & Dev,US EPA, Hampton, VA 23665 USA. RP Pierce, RB (reprint author), NOAA, NESDIS, Adv Satellite Prod Branch, Ctr Satellite Applicat & Res,Cooperat Res Program, 1225 W Dayton St, Madison, WI 53706 USA. EM brad.pierce@noaa.gov RI Pierce, Robert Bradley/F-5609-2010; Ryerson, Tom/C-9611-2009; Thompson, Anne /C-3649-2014 OI Pierce, Robert Bradley/0000-0002-2767-1643; Thompson, Anne /0000-0002-7829-0920 FU U.S. Department of Energy [DE-AC02-05CH11231] FX Thanks go to Bruce Doddridge of the National Aeronautics and Space Administration, Tropospheric Chemistry Program, and Fred Fehsenfeld of the National Oceanic and Atmospheric Administration Earth Systems Research Laboratory for coordinating the NASA involvement in the TexAQS II field mission. Thanks go to an anonymous reviewer for suggesting the sensitivity studies used to examine the role of intraregional transport during the Houston and Dallas high-ozone days. Support for IONS-06 and RAQMS came from the NASA Tropospheric Chemistry Program. The views, opinions, and findings contained in this report are those of the author(s) and should not be construed as an official National Oceanic and Atmospheric Administration or U. S. Government position, policy, or decision. This research used resources of the National Energy Research Scientific Computing Center, which is supported by the Office of Science of the U.S. Department of Energy under contract DE-AC02-05CH11231. NR 39 TC 21 Z9 21 U1 4 U2 12 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD MAY 23 PY 2009 VL 114 AR D00F09 DI 10.1029/2008JD011337 PG 14 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 449XL UT WOS:000266364000004 ER PT J AU Kuznetsova, MM Sibeck, DG Hesse, M Wang, Y Rastaetter, L Toth, G Ridley, A AF Kuznetsova, M. M. Sibeck, D. G. Hesse, M. Wang, Y. Rastaetter, L. Toth, G. Ridley, A. TI Cavities of weak magnetic field strength in the wake of FTEs: Results from global magnetospheric MHD simulations SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID FLUX-TRANSFER EVENTS; MAGNETOPAUSE; GENERATION; FRAMEWORK AB We use the global magnetohydrodynamic (MHD) code BATS-R-US to model multipoint observations of Flux Transfer Event (FTE) signatures. Simulations with high spatial and temporal resolution predict that cavities of weak magnetic field strength protruding into the magnetosphere trail FTEs. These predictions are consistent with recently reported multi-point Cluster observations of traveling magnetopause erosion regions (TMERs). Citation: Kuznetsova, M. M., D. G. Sibeck, M. Hesse, Y. Wang, L. Rastaetter, G. Toth, and A. Ridley (2009), Cavities of weak magnetic field strength in the wake of FTEs: Results from global magnetospheric MHD simulations, Geophys. Res. Lett., 36, L10104, doi: 10.1029/2009GL037489. C1 [Kuznetsova, M. M.; Sibeck, D. G.; Hesse, M.; Wang, Y.; Rastaetter, L.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Toth, G.; Ridley, A.] Univ Michigan, CSEM, Ann Arbor, MI 48109 USA. RP Kuznetsova, MM (reprint author), NASA, Goddard Space Flight Ctr, Code 674, Greenbelt, MD 20771 USA. EM maria.m.kuznetsova@nasa.gov RI Ridley, Aaron/F-3943-2011; Hesse, Michael/D-2031-2012; Sibeck, David/D-4424-2012; Rastaetter, Lutz/D-4715-2012; Kuznetsova, Maria/F-6840-2012; Toth, Gabor/B-7977-2013; NASA MMS, Science Team/J-5393-2013 OI Ridley, Aaron/0000-0001-6933-8534; Rastaetter, Lutz/0000-0002-7343-4147; Toth, Gabor/0000-0002-5654-9823; NASA MMS, Science Team/0000-0002-9504-5214 NR 20 TC 7 Z9 7 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 MAY 22 PY 2009 VL 36 AR L10104 DI 10.1029/2009GL037489 PG 5 WC Geosciences, Multidisciplinary SC Geology GA 449XD UT WOS:000266363200003 ER PT J AU Kishcha, P Starobinets, B Kalashnikova, O Long, CN Alpert, P AF Kishcha, P. Starobinets, B. Kalashnikova, O. Long, C. N. Alpert, P. TI Variations of meridional aerosol distribution and solar dimming SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID IMAGING SPECTRORADIOMETER MISR; MODIS; RADIATION; CLOUD; OCEAN; RETRIEVALS; SURFACE; TRENDS; CONSEQUENCES; CLIMATE AB Meridional distribution of aerosol optical thickness (AOT) over the ocean was analyzed by using the 8-year MISR and MODIS-Terra data sets from March 2000 to February 2008, as well as the 5-year MODIS-Aqua data set from July 2002 to June 2007. The three satellite sensors show that there was a pronounced meridional aerosol asymmetry. It was found that there were strong seasonal variations in the meridional aerosol asymmetry: it was most pronounced in the April-July months. There was no noticeable asymmetry during the season from September to December. The Northern Hemisphere, where the main sources of natural and anthropogenic aerosols are located, contributed to the formation of noticeable aerosol asymmetry. During the season of pronounced hemispheric aerosol asymmetry, an increase in AOT was observed over the Northern Hemisphere, while a decrease in AOT was observed over the Southern Hemisphere. At midlatitudes in the Northern Hemisphere (30-60 degrees N), the main contribution to seasonal variations of AOT over the ocean was made by Pacific Ocean aerosols. At low latitudes in the Northern Hemisphere (0-30 degrees N), aerosols over the Atlantic Ocean contributed to seasonal variations of AOT more significantly than aerosols over the Pacific Ocean. During the 8-year period under consideration, the brightening phenomenon, detected over the land, was not observed over the ocean at midlatitudes 30-60 degrees N in cloudless conditions. C1 [Kishcha, P.; Starobinets, B.; Alpert, P.] Tel Aviv Univ, Dept Geophys & Planetary Sci, IL-69978 Tel Aviv, Israel. [Kalashnikova, O.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Long, C. N.] Pacific NW Natl Lab, Richland, WA 99352 USA. RP Kishcha, P (reprint author), Tel Aviv Univ, Dept Geophys & Planetary Sci, IL-69978 Tel Aviv, Israel. EM pavel@cyclone.tau.ac.il FU GLOWA-Jordan River BMBF (Germany)-MOST (Israel) [1946]; U. S. Department of Energy; NASA Earth Sciences Division FX We gratefully acknowledge L. Remer, R. Levy, and Y. Agnon for their helpful discussion, the GES-DISC Interactive Online Visualization and Analysis Infrastructure (Giovanni) for providing MODIS data, the NASA Langley Research Center Atmospheric Sciences Data Center for providing MISR data, and NOAA/OAR/ESRL Physical Science Division for providing NCEP reanalysis data from their Web site (http://www.cdc.noaa.gov/). This study was supported by the GLOWA-Jordan River BMBF (Germany)-MOST (Israel) project, the BMBF-MOST grant 1946 on global change, and the Israeli Science Foundation (ISF) grant 764/06. C. N. Long acknowledges the support of the Climate Change Research Division of the U. S. Department of Energy as part of the Atmospheric Radiation Measurement (ARM) Program. The work of O. Kalashnikova is supported by a grant from the NASA Earth Sciences Division, Climate and Radiation program, under H. Maring. The work of O. Kalashnikova was performed at the Jet Propulsion Laboratory, California Institute of Technology, under contract with NASA. NR 49 TC 12 Z9 12 U1 0 U2 3 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 MAY 22 PY 2009 VL 114 AR D00D14 DI 10.1029/2008JD010975 PG 14 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 449XK UT WOS:000266363900001 ER PT J AU van Diedenhoven, B Fridlind, AM Ackerman, AS Eloranta, EW McFarquhar, GM AF van Diedenhoven, B. Fridlind, A. M. Ackerman, A. S. Eloranta, E. W. McFarquhar, G. M. TI An evaluation of ice formation in large-eddy simulations of supercooled Arctic stratocumulus using ground-based lidar and cloud radar SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID SINGLE-SCATTERING PROPERTIES; BOUNDARY-LAYER; RESOLVING SIMULATIONS; STRATIFORM CLOUDS; FORMING NUCLEI; BEAUFORT SEA; CRYSTALS; PARTICLES; MODEL; MICROWAVE AB In order to evaluate possible ice formation processes in mixed phase Arctic stratocumulus, we compare measurements of radar reflectivity and Doppler velocity and lidar backscatter coefficient and circular depolarization ratio with the corresponding quantities computed from large-eddy simulations (LES). The measurements are taken from the Millimeter Cloud Radar and the Arctic High Spectral Resolution Lidar during the Mixed-Phase Arctic Cloud Experiment in October 2004. Lidar depolarization, computed from LES results including well-known ice formation and multiplication processes and measured ambient ice nuclei (IN), is near 0%, indicating negligible ice formation, whereas measured median depolarization is 84%, indicating strong ice formation, consistent with in situ aircraft measurements. Reducing ice particle fall speeds, increasing IN concentrations, or introducing a surface source of IN does not sufficiently increase the simulated depolarization values and/or results in poor agreement of other simulated parameters with the measurements. Introducing additional hypothetical ice formation processes (i.e., formation of IN from evaporating drops, freezing of evaporation drops, or droplet freezing rates per unit surface or volume) generally brings all investigated parameters into relatively close agreement with the radar and lidar measurements. These results provide additional evidence for the existence of one or more unestablished ice formation processes in Arctic stratocumulus. C1 [van Diedenhoven, B.] Columbia Univ, Ctr Climate Syst Res, New York, NY 10027 USA. [van Diedenhoven, B.; Fridlind, A. M.; Ackerman, A. S.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA. [Eloranta, E. W.] Univ Wisconsin, Ctr Space Sci & Engn, Madison, WI 53706 USA. [McFarquhar, G. M.] Univ Illinois, Dept Atmospher Sci, Urbana, IL 61801 USA. RP van Diedenhoven, B (reprint author), Columbia Univ, Ctr Climate Syst Res, New York, NY 10027 USA. EM bvandiedenhoven@giss.nasa.gov RI Ackerman, Andrew/D-4433-2012; Fridlind, Ann/E-1495-2012; van Diedenhoven, Bastiaan/A-2002-2013; OI Ackerman, Andrew/0000-0003-0254-6253; van Diedenhoven, Bastiaan/0000-0001-5622-8619; McFarquhar, Greg/0000-0003-0950-0135 FU NASA [06-EOS/06-100]; Department of Energy [DE-AI02-06ER64173] FX This material is based upon work supported by NASA under grant 06-EOS/06-100 issued through the Science Mission Directorate, Earth Science Division, and by the Department of Energy under Interagency Agreement DE-AI02-06ER64173 issued through the Office of Science, Office of Biological and Environmental Research. M-PACE in situ data and MMCR data were obtained from the Atmospheric Radiation Measurement (ARM) Program sponsored by the U. S. Department of Energy, Office of Science, Office of Biological and Environmental Research, Environmental Sciences Division. AHSRL data were obtained from the University of Wisconsin. Computational resources were provided by the NASA Advanced Supercomputing Division through the NASA High-End Computing Program. We thank Michael Mishchenko for valuable conversations. We are grateful for contributions from three anonymous reviewers. NR 67 TC 7 Z9 7 U1 2 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 MAY 22 PY 2009 VL 114 AR D10203 DI 10.1029/2008JD011198 PG 18 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 449XK UT WOS:000266363900003 ER PT J AU Squyres, SW Knoll, AH Arvidson, RE Ashley, JW Bell, JF Calvin, WM Christensen, PR Clark, BC Cohen, BA de Souza, PA Edgar, L Farrand, WH Fleischer, I Gellert, R Golombek, MP Grant, J Grotzinger, J Hayes, A Herkenhoff, KE Johnson, JR Jolliff, B Klingelhofer, G Knudson, A Li, R Mccoy, TJ McLennan, SM Ming, DW Mittlefehldt, DW Morris, RV Rice, JW Schroder, C Sullivan, RJ Yen, A Yingst, RA AF Squyres, S. W. Knoll, A. H. Arvidson, R. E. Ashley, J. W. Bell, J. F., III Calvin, W. M. Christensen, P. R. Clark, B. C. Cohen, B. A. de Souza, P. A., Jr. Edgar, L. Farrand, W. H. Fleischer, I. Gellert, R. Golombek, M. P. Grant, J. Grotzinger, J. Hayes, A. Herkenhoff, K. E. Johnson, J. R. Jolliff, B. Klingelhoefer, G. Knudson, A. Li, R. McCoy, T. J. McLennan, S. M. Ming, D. W. Mittlefehldt, D. W. Morris, R. V. Rice, J. W., Jr. Schroeder, C. Sullivan, R. J. Yen, A. Yingst, R. A. TI Exploration of Victoria Crater by the Mars Rover Opportunity SO SCIENCE LA English DT Article ID MERIDIANI-PLANUM; BURNS FORMATION AB The Mars rover Opportunity has explored Victoria crater, a similar to 750-meter eroded impact crater formed in sulfate-rich sedimentary rocks. Impact-related stratigraphy is preserved in the crater walls, and meteoritic debris is present near the crater rim. The size of hematite-rich concretions decreases up-section, documenting variation in the intensity of groundwater processes. Layering in the crater walls preserves evidence of ancient wind-blown dunes. Compositional variations with depth mimic those similar to 6 kilometers to the north and demonstrate that water-induced alteration at Meridiani Planum was regional in scope. C1 [Squyres, S. W.; Bell, J. F., III; Sullivan, R. J.] Cornell Univ, Dept Astron, Ithaca, NY 14853 USA. [Knoll, A. H.] Harvard Univ, Bot Museum, Cambridge, MA 02138 USA. [Arvidson, R. E.; Jolliff, B.] Washington Univ, Dept Earth & Planetary Sci, St Louis, MO 63031 USA. [Ashley, J. W.; Christensen, P. R.; Knudson, A.; Rice, J. W., Jr.] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85287 USA. [Calvin, W. M.] Univ Nevada, Reno, NV 89557 USA. [Clark, B. C.] Lockheed Martin Corp, Littleton, CO 80127 USA. [Cohen, B. A.] NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA. [de Souza, P. A., Jr.] CSIRO, Tasmanian Informat & Commun Technol Ctr, Hobart, Tas 7000, Australia. [Edgar, L.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. [Farrand, W. H.] Space Sci Inst, Boulder, CO 80301 USA. [Fleischer, I.; Klingelhoefer, G.; Schroeder, C.] Johannes Gutenberg Univ Mainz, Inst Anorgan & Analyt Chem, Mainz, Germany. [Gellert, R.] Univ Guelph, Dept Phys, Guelph, ON N1G 2W1, Canada. [Golombek, M. P.; Yen, A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Grant, J.] Smithsonian Inst, Ctr Earth & Planetary Studies, Washington, DC 20560 USA. [Herkenhoff, K. E.; Johnson, J. R.] US Geol Survey, Flagstaff, AZ 86001 USA. [Li, R.] Ohio State Univ, Dept Civil & Environm Engn & Geodet Sci, Columbus, OH 43210 USA. [McCoy, T. J.] Smithsonian Inst, Natl Museum Nat Hist, Dept Mineral Sci, Washington, DC 20560 USA. [McLennan, S. M.] SUNY Stony Brook, Dept Geosci, Stony Brook, NY 11794 USA. [Ming, D. W.; Mittlefehldt, D. W.; Morris, R. V.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. [Yingst, R. A.] Univ Wisconsin, Green Bay, WI 54311 USA. RP Squyres, SW (reprint author), Cornell Univ, Dept Astron, Space Sci Bldg, Ithaca, NY 14853 USA. EM squyres@astro.cornell.edu RI de Souza, Paulo/B-8961-2008; Schroder, Christian/B-3870-2009; Centre, TasICT/D-1212-2011; Hayes, Alexander/P-2024-2014; Johnson, Jeffrey/F-3972-2015 OI de Souza, Paulo/0000-0002-0091-8925; Schroder, Christian/0000-0002-7935-6039; Hayes, Alexander/0000-0001-6397-2630; FU NASA FX This research was carried out for the Jet Propulsion Laboratory, California Institute of Technology, under a contract with NASA. NR 23 TC 76 Z9 76 U1 0 U2 24 PU AMER ASSOC ADVANCEMENT SCIENCE PI WASHINGTON PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 USA SN 0036-8075 EI 1095-9203 J9 SCIENCE JI Science PD MAY 22 PY 2009 VL 324 IS 5930 BP 1058 EP 1061 DI 10.1126/science.1170355 PG 4 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 448EU UT WOS:000266246700038 PM 19461001 ER PT J AU Cao, L Bala, G Caldeira, K Nemani, R Ban-Weiss, G AF Cao, Long Bala, Govindasamy Caldeira, Ken Nemani, Ramakrishna Ban-Weiss, George TI Climate response to physiological forcing of carbon dioxide simulated by the coupled Community Atmosphere Model (CAM3.1) and Community Land Model (CLM3.0) SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID SYSTEM MODEL; PLANT; CO2; EVAPOTRANSPIRATION; SURFACE; RUNOFF; GCM AB Increasing concentrations of atmospheric CO(2) decrease stomatal conductance of plants and thus suppress canopy transpiration. The climate response to this CO(2)-physiological forcing is investigated using the Community Atmosphere Model version 3.1 coupled to Community Land Model version 3.0. In response to the physiological effect of doubling CO(2), simulations show a decrease in canopy transpiration of 8%, a mean warming of 0.1K over the land surface, and negligible changes in the hydrological cycle. These climate responses are much smaller than what were found in previous modeling studies. This is largely a result of unrealistic partitioning of evapotranspiration in our model control simulation with a greatly underestimated contribution from canopy transpiration and overestimated contributions from canopy and soil evaporation. This study highlights the importance of a realistic simulation of the hydrological cycle, especially the individual components of evapotranspiration, in reducing the uncertainty in our estimation of climatic response to CO(2)-physiological forcing. Citation: Cao, L., G. Bala, K. Caldeira, R. Nemani, and G. Ban-Weiss (2009), Climate response to physiological forcing of carbon dioxide simulated by the coupled Community Atmosphere Model (CAM3.1) and Community Land Model (CLM3.0), Geophys. Res. Lett., 36, L10402, doi: 10.1029/2009GL037724. C1 [Cao, Long; Caldeira, Ken; Ban-Weiss, George] Carnegie Inst, Dept Global Ecol, Stanford, CA 94305 USA. [Bala, Govindasamy] Indian Inst Sci, Ctr Atmospher & Ocean Sci, Bangalore 560012, Karnataka, India. [Nemani, Ramakrishna] NASA, Ames Res Ctr, Div Earth Sci, Moffett Field, CA 94035 USA. [Bala, Govindasamy] Indian Inst Sci, Divecha Ctr Climate Change, Bangalore 560012, Karnataka, India. RP Cao, L (reprint author), Carnegie Inst, Dept Global Ecol, 260 Panama St, Stanford, CA 94305 USA. EM longcao@stanford.edu RI Caldeira, Ken/E-7914-2011; OI Ban-Weiss, George/0000-0001-8211-2628 NR 20 TC 23 Z9 24 U1 0 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 MAY 21 PY 2009 VL 36 AR L10402 DI 10.1029/2009GL037724 PG 5 WC Geosciences, Multidisciplinary SC Geology GA 449XC UT WOS:000266363000004 ER PT J AU Howell, SEL Duguay, CR Markus, T AF Howell, Stephen E. L. Duguay, Claude R. Markus, Thorsten TI Sea ice conditions and melt season duration variability within the Canadian Arctic Archipelago: 1979-2008 SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article AB Sea ice conditions and melt season duration within the Canadian Arctic Archipelago (CAA) were investigated from 1979-2008. The CAA is exhibiting statistically significant decreases in average September total sea ice area at -8.7% decade(-1). The melt season duration within the CAA is increasing significantly at 7 days decade(-1). 2008 represented the longest melt season duration within the CAA over the satellite record at 129 days. Average September multi-year ice (MYI) area is decreasing at -6.4% decade(-1) but has yet to reach statistical significance as a result of increasing MYI dynamic import from the Arctic Ocean. Results also find that the Western Parry Channel (WPC) region of the Northwest Passage (NWP) will continue to be susceptible to MYI as the transition to a summer-time sea ice free Arctic continues. The processes responsible for the temporary clearing of the WPC region of the NWP in 2007 were also identified. Citation: Howell, S. E. L., C. R. Duguay, and T. Markus (2009), Sea ice conditions and melt season duration variability within the Canadian Arctic Archipelago: 1979-2008, Geophys. Res. Lett., 36, L10502, doi: 10.1029/2009GL037681. C1 [Howell, Stephen E. L.; Duguay, Claude R.] Univ Waterloo, Interdisciplinary Ctr Climate Change, Waterloo, ON N2L 3G1, Canada. [Howell, Stephen E. L.; Duguay, Claude R.] Univ Waterloo, Dept Geog & Environm Management, Waterloo, ON N2L 3G1, Canada. [Markus, Thorsten] NASA, Goddard Space Flight Ctr, Cryospher Sci Branch, Greenbelt, MD 20771 USA. RP Howell, SEL (reprint author), Univ Waterloo, Interdisciplinary Ctr Climate Change, Waterloo, ON N2L 3G1, Canada. EM showell@uwaterloo.ca RI Duguay, Claude/G-5682-2011; Markus, Thorsten/D-5365-2012 OI Duguay, Claude/0000-0002-1044-5850; FU Natural Sciences and Engineering Research Council (NSERC) FX This research was supported by a Natural Sciences and Engineering Research Council (NSERC) Post Doctoral Fellowship to S. Howell and NSERC Discovery grant to C. Duguay. NR 14 TC 48 Z9 49 U1 2 U2 13 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD MAY 21 PY 2009 VL 36 AR L10502 DI 10.1029/2009GL037681 PG 6 WC Geosciences, Multidisciplinary SC Geology GA 449XC UT WOS:000266363000003 ER PT J AU Kearney, C Watson, IM Bluth, GJS Carn, S Realmuto, VJ AF Kearney, C. Watson, I. M. Bluth, G. J. S. Carn, S. Realmuto, V. J. TI A comparison of thermal infrared and ultraviolet retrievals of SO2 in the cloud produced by the 2003 Al-Mishraq State sulfur plant fire SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID OZONE MAPPING SPECTROMETER; DIOXIDE; VOLCANOS AB The detection of SO2 plumes by space-based sensors has been demonstrated in the UV and TIR. However, the relationship between these retrieval techniques is poorly constrained. In this paper we compare near-coincidental EP TOMS and MODIS data of a near-pure SO2 plume from the Al-Mishraq State sulfur plant fire on 29 June 2003. We resampled the MODIS data to the spatial resolution of EP TOMS in order to compare the two SO2 retrievals at the pixel scale. EP TOMS and MODIS return SO2 total tonnages of 103 and 118 kt, respectively. Overall, the agreement between the techniques on a pixel scale ranges between 10% to greater than 90% with no discernible spatial pattern. The variable agreement between the two retrievals is likely the result of differences in spatial resolution, presence of sulfates, and variations in plume height with distance from the fire. Citation: Kearney, C., I. M. Watson, G. J. S. Bluth, S. Carn, and V. J. Realmuto (2009), A comparison of thermal infrared and ultraviolet retrievals of SO2 in the cloud produced by the 2003 Al-Mishraq State sulfur plant fire, Geophys. Res. Lett., 36, L10807, doi: 10.1029/2009GL038215. C1 [Kearney, C.; Watson, I. M.] Univ Bristol, Dept Earth Sci, Bristol BS8 1RJ, Avon, England. [Watson, I. M.; Bluth, G. J. S.] Michigan Technol Univ, Houghton, MI 49931 USA. [Carn, S.] Univ Maryland Baltimore Cty, Joint Ctr Earth Syst Technol, Catonsville, MD 21228 USA. [Realmuto, V. J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Kearney, C (reprint author), Univ Bristol, Dept Earth Sci, Queens Rd, Bristol BS8 1RJ, Avon, England. EM c.kearney@bristol.ac.uk RI Watson, Matt/E-5236-2011 OI Watson, Matt/0000-0001-9198-2203 NR 10 TC 6 Z9 6 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 MAY 21 PY 2009 VL 36 AR L10807 DI 10.1029/2009GL038215 PG 5 WC Geosciences, Multidisciplinary SC Geology GA 449XC UT WOS:000266363000005 ER PT J AU Serke, DJ Politovich, MK Reehorst, AL Gaydos, A AF Serke, David J. Politovich, Marcia K. Reehorst, Andrew L. Gaydos, Andy TI Use of X-band radars to support the detection of in-flight icing hazards SO JOURNAL OF APPLIED REMOTE SENSING LA English DT Article DE NASA Icing Remote Sensing System; Alliance Icing Research Study-II; in-flight icing; X-band radar; twin otter aircraft ID WATER AB The NASA Icing Remote Sensing System was operated for the Alliance Icing Research Study II field program during the winter of 2003 around Montreal, Canada and around Cleveland, Ohio during the winter of 2005. Icing research aircraft flights from these field programs provided verification data on liquid water content, air temperature and also cloud particle imagery and distributions. The purpose of this work is to show that the NASA Icing Remote Sensing System X-band radar reflectivity profiles could be used beyond merely defining vertical cloud boundaries, by operationally deriving a qualitative small drop icing hazard warning flag. Several case studies are presented which depict a variety of synoptic weather scenarios. These cases demonstrate that X-band reflectivities below-10 dBZ and above the minimum detectable are uniquely indicative of a particle population dominated by small, liquid droplets. A discussion is included for each case on how an in-flight icing hazard flag from the radar reflectivity profile would improve the operational hazard detection system. Comparison of the NASA Icing Remote Sensing System's X-band radar data to a nearby similar X-band from McGill University is done to ensure data quality and consistency. C1 [Serke, David J.; Politovich, Marcia K.; Gaydos, Andy] Natl Ctr Atmospher Res, Res Applicat Lab, Boulder, CO 80301 USA. [Reehorst, Andrew L.] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. RP Serke, DJ (reprint author), Natl Ctr Atmospher Res, Res Applicat Lab, 3450 Mitchell Lane, Boulder, CO 80301 USA. EM serke@ucar.edu; marciap@ucar.edu; Andrew.L.Reehorst@nasa.gov; gaydos@ucar.edu FU NASA Aviation Safety Program, Integrated Intelligent Flight Deck Support FX This work supports the NASA Aviation Safety Program, Integrated Intelligent Flight Deck Support. The views expressed in this document represents the opinion of the authors and do not necessarily represent the official policy or position of NASA. The authors would like Dr. Jothiram Vivekanandan and Frank McDonough for their comments, which were a great help in preparing this manuscript. NR 9 TC 0 Z9 0 U1 0 U2 5 PU SPIE-SOC PHOTOPTICAL INSTRUMENTATION ENGINEERS PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98225 USA SN 1931-3195 J9 J APPL REMOTE SENS JI J. Appl. Remote Sens. PD MAY 21 PY 2009 VL 3 AR 033532 DI 10.1117/1.3153335 PG 13 WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic Technology SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science & Photographic Technology GA 520WO UT WOS:000271880400002 ER PT J AU Nair, NG Blanco, M West, W Weise, FC Greenbaum, S Reddy, VP AF Nair, Nanditha G. Blanco, Mario West, William Weise, F. Christoph Greenbaum, Steve Reddy, V. Prakash TI Fluorinated Boroxin-Based Anion Receptors for Lithium Ion Batteries: Fluoride Anion Binding, Ab Initio Calculations, and Ionic Conductivity Studies SO JOURNAL OF PHYSICAL CHEMISTRY A LA English DT Article ID TRIS(PENTAFLUOROPHENYL) BORANE; ELECTROLYTES; COMPLEXES; DME AB Novel fluorinated boroxines, tris(2,6-difluorophenyl)boroxin (DF), tris(2,4,6-trifluorophenyl)boroxin (TF), and tris(pentafluorophenyl)boroxin (PF), have been investigated for potential applications in lithium ion batteries through fluoride anion binding, ab initio calculations, and ionic conductivity measurements. Structures of the fluorinated boroxines and boroxin-fluoride complexes have been confirmed by comparing their F-19 and B-11 NMR chemical shifts with those obtained by the DFT-GIAO method. The stoichiometry of the fluoride anion binding to these boroxines has been shown to be 1:1 using F-19 NMR and UV-vis spectroscopy. UV-vis spectroscopic studies show the coexistence of more than one complex, in addition to the 1:1 complex, for perfluorinated boroxin, PF. DFT calculations (B3LYP/6-311G**) show that the fluoride ion complex of DF prefers unsymmetrical, covalently bound structure (7) over the symmetrically bridged species (10) by 12.5 kcal/mol. Rapid equilibration of the fluoride anion among the three borons in these boroxines results in a single F-19 NMR absorption for all of the aromatic ortho- or para-fluorines at ambient temperature. The effect of these anion receptors on lithium ion conductivities was also explored for potential applications in dual ion intercalating lithium batteries. C1 [Blanco, Mario] CALTECH, Dept Chem, Pasadena, CA 91109 USA. [Nair, Nanditha G.; Reddy, V. Prakash] Missouri Univ Sci & Technol, Dept Chem, Rolla, MO 65409 USA. [West, William] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Weise, F. Christoph; Greenbaum, Steve] CUNY Hunter Coll, New York, NY 10021 USA. RP Blanco, M (reprint author), CALTECH, Dept Chem, Pasadena, CA 91109 USA. EM preddy@mst.edu FU Army Research Office. N.G.N; Missouri ST FX The work described here was carried out, in part, at the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. Authors W.C.W. and M.B. gratefully acknowledge the support of this work by the Army Research Office. N.G.N. gratefully acknowledges graduate fellowship from Missouri S&T. NR 28 TC 17 Z9 17 U1 3 U2 25 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 1089-5639 J9 J PHYS CHEM A JI J. Phys. Chem. A PD MAY 21 PY 2009 VL 113 IS 20 BP 5918 EP 5926 DI 10.1021/jp901952t PG 9 WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical SC Chemistry; Physics GA 446AV UT WOS:000266093500014 PM 19397307 ER PT J AU Inam, SC Townsend, LJ McBride, VA Baykal, A Coe, MJ Corbet, RHD AF Inam, S. C. Townsend, L. J. McBride, V. A. Baykal, A. Coe, M. J. Corbet, R. H. D. TI RXTE-PCA observations of XMMU J054134.7-682550 SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE accretion, accretion discs; stars: neutron; pulsars: individual: XMMU J054134.7-682550; X-rays: binaries ID X-RAY PULSAR; ATMOSPHERES; LUMINOSITY; ACCRETION; BINARIES AB We analysed Rossi X-ray Timing Explorer Proportional Counter Array observations of a recent outburst of the X-ray pulsar XMMU J054134.7-682550. We calculated the pulse frequency history of the source. We found no sign of a binary companion. The source spins up when the X-ray flux is higher, with a correlation between the spin-up rate and X-ray flux, which may be interpreted as a sign of an accretion disc. On the other hand, the source was found to have an almost constant spin frequency when the X-ray flux is lower without any clear sign of a spin-down episode. The decrease in pulsed fraction with decreasing X-ray flux was interpreted as a sign of accretion geometry change, but we did not find any evidence of a transition from accretor to propeller regimes. The source was found to have variable pulse profiles. Two peaks in pulse profiles were usually observed. We studied the X-ray spectral evolution of the source throughout the observation. Pulse-phase-resolved analysis does not provide any further evidence for a cyclotron line, but may suggest a slight variation of intensity and width of the 6.4 keV iron line with phase. C1 [Inam, S. C.] Baskent Univ, Dept Elect & Elect Engn, TR-06530 Ankara, Turkey. [Townsend, L. J.; McBride, V. A.; Coe, M. J.] Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England. [Baykal, A.] Middle E Tech Univ, Dept Phys, TR-06531 Ankara, Turkey. [Corbet, R. H. D.] Univ Maryland, NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Inam, SC (reprint author), Baskent Univ, Dept Elect & Elect Engn, TR-06530 Ankara, Turkey. EM inam@baskent.edu.tr; altan@astroa.physics.metu.edu.tr FU TUBITAK; Scientific and Technological Research Council of Turkey [106T040]; EU FP6 Transfer of Knowledge Project [MTKD-CT-2006-042722]; Mayflower grant; School of Physics and Astronomy FX SCI and AB acknowledge support from TUBITAK, the Scientific and Technological Research Council of Turkey through project 106T040 and EU FP6 Transfer of Knowledge Project 'Astrophysics of Neutron Stars' (MTKD-CT-2006-042722). We would like to thank Jorn Wilms and the IAAT library for the IDL routines used in this analysis. LJT is funded by a Mayflower grant and would like to thank the School of Physics and Astronomy for their support. NR 26 TC 8 Z9 8 U1 0 U2 1 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD MAY 21 PY 2009 VL 395 IS 3 BP 1662 EP 1668 DI 10.1111/j.1365-2966.2009.14659.x PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 443UJ UT WOS:000265936000045 ER PT J AU Hernan-Caballero, A Perez-Fournon, I Hatziminaoglou, E Afonso-Luis, A Rowan-Robinson, M Rigopoulou, D Farrah, D Lonsdale, CJ Babbedge, T Clements, D Serjeant, S Pozzi, F Vaccari, M Montenegro-Montes, FM Valtchanov, I Gonzalez-Solares, E Oliver, S Shupe, D Gruppioni, C Vila-Vilaro, B Lari, C La Franca, F AF Hernan-Caballero, A. Perez-Fournon, I. Hatziminaoglou, E. Afonso-Luis, A. Rowan-Robinson, M. Rigopoulou, D. Farrah, D. Lonsdale, C. J. Babbedge, T. Clements, D. Serjeant, S. Pozzi, F. Vaccari, M. Montenegro-Montes, F. M. Valtchanov, I. Gonzalez-Solares, E. Oliver, S. Shupe, D. Gruppioni, C. Vila-Vilaro, B. Lari, C. La Franca, F. TI Mid-infrared spectroscopy of infrared-luminous galaxies at z similar to 0.5-3 SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Review DE galaxies: active; galaxies: high-redshift; quasars: general; galaxies: starburst ID ACTIVE GALACTIC NUCLEI; SPECTRAL ENERGY-DISTRIBUTIONS; SPITZER-SPACE-TELESCOPE; POLYCYCLIC AROMATIC-HYDROCARBONS; AREA ISO SURVEY; ULTRALUMINOUS IRAS GALAXIES; DIFFUSE INTERSTELLAR-MEDIUM; PALOMAR-GREEN QUASARS; STAR-FORMING GALAXIES; DIGITAL SKY SURVEY AB We present results on low-resolution mid-infrared (MIR) spectra of 70 IR-luminous galaxies obtained with the infrared spectrograph (IRS) onboard Spitzer. We selected sources from the European Large Area Infrared Survey with S(15) > 0.8 mJy and photometric or spectroscopic z > 1. About half of the samples are quasi-stellar objects (QSOs) in the optical, while the remaining sources are galaxies, comprising both obscured active galactic nuclei (AGN) and starbursts. Redshifts were obtained from optical spectroscopy, photometric redshifts and the IRS spectra. The later turn out to be reliable for obscured and/or star-forming sources, thus becoming an ideal complement to optical spectroscopy for redshift estimation. We estimate monochromatic luminosities at several rest-frame wavelengths, equivalent widths and luminosities for the polycyclic aromatic hydrocarbon (PAH) features, and strength of the silicate feature in individual spectra. We also estimate integrated 8-1000 mu m IR luminosities via spectral energy distribution fitting to MIR and far-IR (FIR) photometry from the Spitzer Wide-Area Infrared Extragalactic survey and the MIR spectrum. Based on these measurements, we classify the spectra using well-known IR diagnostics, as well as a new one that we propose, into three types of source: those dominated by an unobscured AGN, mostly corresponding to optical quasars (QSOs), those dominated by an obscured AGN and starburst-dominated sources. Starbursts concentrate at z similar to 0.6-1.0 favoured by the shift of the 7.7-mu m PAH band into the selection 15-mu m band, while AGN spread over the 0.5 < z < 3.1 range. Star formation rates (SFR) are estimated for individual sources from the luminosity of the PAH features. An estimate of the average PAH luminosity in QSOs and obscured AGN is obtained from the composite spectrum of all sources with reliable redshifts. The estimated mean SFR in the QSOs is 50-100M(circle dot) yr(-1), but the implied FIR luminosity is 3-10 times lower than that obtained from stacking analysis of the FIR photometry, suggesting destruction of the PAH carriers by energetic photons from the AGN. The SFR estimated in obscured AGN is two to three times higher than in QSOs of similar MIR luminosity. This discrepancy might not be due to luminosity effects or selection bias alone, but could instead indicate a connection between obscuration and star formation. However, the observed correlation between silicate absorption and the slope of the NIR to MIR spectrum is compatible with the obscuration of the AGN emission in these sources being produced in a dust torus. C1 [Hernan-Caballero, A.; Perez-Fournon, I.; Afonso-Luis, A.; Montenegro-Montes, F. M.] Inst Astrofis Canarias, E-38200 San Cristobal la Laguna, Spain. [Hatziminaoglou, E.] European So Observ, D-85748 Garching, Germany. [Rowan-Robinson, M.; Babbedge, T.; Clements, D.; Vaccari, M.; Valtchanov, I.] Univ London Imperial Coll Sci Technol & Med, Astrophys Grp, Blackett Lab, London SW7 2BW, England. [Rigopoulou, D.] Univ Oxford, Dept Phys, Oxford OX1 3RH, England. [Farrah, D.] Cornell Univ, Dept Astron, Ithaca, NY 14853 USA. [Farrah, D.] Univ Sussex, Ctr Astron, Dept Phys & Astron, Brighton BN1 9QJ, E Sussex, England. [Lonsdale, C. J.] CALTECH, Infrared Proc & Anal Ctr, Pasadena, CA 91125 USA. [Serjeant, S.] Univ Kent, Ctr Astrophys & Planetary Sci, Sch Phys Sci, Canterbury CT2 7NR, Kent, England. [Pozzi, F.] Univ Bologna, Dipartimento Astron, I-40127 Bologna, Italy. [Vaccari, M.] Univ Padua, Dipartimento Astron, I-35122 Padua, Italy. [Montenegro-Montes, F. M.; Lari, C.] INAF, Ist Radioastron, I-40129 Bologna, Italy. [Valtchanov, I.] ESA European Space Astron Ctr, Madrid, Spain. [Gonzalez-Solares, E.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. Spitzer Sci Ctr, Jet Prop Lab, Pasadena, CA 91125 USA. [Gruppioni, C.] INAF, Osservatorio Astron Bologna, I-40127 Bologna, Italy. [Vila-Vilaro, B.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [La Franca, F.] Univ Roma Tre, Dipartimento Fis, I-00146 Rome, Italy. RP Hernan-Caballero, A (reprint author), Inst Astrofis Canarias, C Via Lactea S-N, E-38200 San Cristobal la Laguna, Spain. EM ahc@iac.es RI La Franca, Fabio/G-9631-2012; Vaccari, Mattia/R-3431-2016; OI Vaccari, Mattia/0000-0002-6748-0577; Montenegro Montes, Francisco Miguel/0000-0002-7430-3771; Gruppioni, Carlotta/0000-0002-5836-4056 FU Spanish Plan Nacional del Espacio [ESP2007-65812-C02-02]; UK PPARC FX We wish to thank the anonymous referee for very useful comments and suggestions. NR 119 TC 47 Z9 47 U1 0 U2 0 PU WILEY-BLACKWELL PUBLISHING, INC PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD MAY 21 PY 2009 VL 395 IS 3 BP 1695 EP 1722 DI 10.1111/j.1365-2966.2009.14660.x PG 28 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 443UJ UT WOS:000265936000047 ER PT J AU Shindell, D AF Shindell, Drew TI Protecting the environment can boost the economy SO NATURE LA English DT Letter C1 NASA, Goddard Inst Space Studies, New York, NY 10025 USA. RP Shindell, D (reprint author), NASA, Goddard Inst Space Studies, 2880 Broadway, New York, NY 10025 USA. EM drew.t.shindell@nasa.gov NR 0 TC 0 Z9 0 U1 1 U2 7 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 0028-0836 J9 NATURE JI Nature PD MAY 21 PY 2009 VL 459 IS 7245 BP 321 EP 321 DI 10.1038/459321b PG 1 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 448DQ UT WOS:000266243700014 PM 19458692 ER PT J AU Rothschild, LJ AF Rothschild, Lynn J. TI EARTH SCIENCE Life battered but unbowed SO NATURE LA English DT Editorial Material ID DIVERSITY; BIOSPHERE; ZIRCONS; ORIGIN; DEEP C1 NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Rothschild, LJ (reprint author), NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. EM lynn.j.rothschild@nasa.gov NR 18 TC 2 Z9 2 U1 1 U2 8 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 0028-0836 J9 NATURE JI Nature PD MAY 21 PY 2009 VL 459 IS 7245 BP 335 EP 336 DI 10.1038/459335a PG 2 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 448DQ UT WOS:000266243700026 PM 19458704 ER PT J AU Fairen, AG Davila, AF Gago-Duport, L Amils, R McKay, CP AF Fairen, Alberto G. Davila, Alfonso F. Gago-Duport, Luis Amils, Ricardo McKay, Christopher P. TI Stability against freezing of aqueous solutions on early Mars SO NATURE LA English DT Article ID CARBON-DIOXIDE CLOUDS; WATER; EARTH; ATMOSPHERES; CLIMATE AB Many features of the Martian landscape are thought to have been formed by liquid water flow(1,2) and water-related mineralogies on the surface of Mars are widespread and abundant(3). Several lines of evidence, however, suggest that Mars has been cold with mean global temperatures well below the freezing point of pure water(4). Martian climate modellers(5,6) considering a combination of greenhouse gases at a range of partial pressures find it challenging to simulate global mean Martian surface temperatures above 273 K, and local thermal sources(7,8) cannot account for the widespread distribution of hydrated and evaporitic minerals throughout the Martian landscape(3). Solutes could depress the melting point of water(9,10) in a frozen Martian environment, providing a plausible solution to the early Mars climate paradox. Here we model the freezing and evaporation processes of Martian fluids with a composition resulting from the weathering of basalts, as reflected in the chemical compositions at Mars landing sites. Our results show that a significant fraction of weathering fluids loaded with Si, Fe, S, Mg, Ca, Cl, Na, K and Al remain in the liquid state at temperatures well below 273 K. We tested our model by analysing the mineralogies yielded by the evolution of the solutions: the resulting mineral assemblages are analogous to those actually identified on the Martian surface. This stability against freezing of Martian fluids can explain saline liquid water activity on the surface of Mars at mean global temperatures well below 273 K. C1 [Fairen, Alberto G.; Davila, Alfonso F.; McKay, Christopher P.] NASA, Ames Res Ctr, Space Sci & Astrobiol Div, Moffett Field, CA 94035 USA. [Gago-Duport, Luis] Univ Vigo, Dept Geociencias Marinas, Vigo 36200, Spain. [Amils, Ricardo] CSIC INTA, Ctr Astrobiol, Madrid 28850, Spain. [Amils, Ricardo] CSIC UAM, Ctr Biol Mol Severo Ochoa, Madrid 28049, Spain. RP Fairen, AG (reprint author), NASA, Ames Res Ctr, Space Sci & Astrobiol Div, Moffett Field, CA 94035 USA. EM alberto.g.fairen@nasa.gov RI Davila, Alfonso/A-2198-2013 OI Davila, Alfonso/0000-0002-0977-9909 FU ORAU-NPP FX Work by A. G. F. and A. F. D. was supported by ORAU-NPP. We thank J. Kasting and J. Kargel for reviews that significantly improved the paper. NR 30 TC 60 Z9 61 U1 2 U2 13 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 0028-0836 J9 NATURE JI Nature PD MAY 21 PY 2009 VL 459 IS 7245 BP 401 EP 404 DI 10.1038/nature07978 PG 4 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 448DQ UT WOS:000266243700040 PM 19458717 ER PT J AU Cordiner, MA Millar, TJ AF Cordiner, M. A. Millar, T. J. TI DENSITY-ENHANCED GAS AND DUST SHELLS IN A NEW CHEMICAL MODEL FOR IRC+10216 SO ASTROPHYSICAL JOURNAL LA English DT Article DE astrochemistry; circumstellar matter; ISM: molecules; stars: individual (IRC+10216) ID ENVELOPE SURROUNDING IRC+10216; CARBON-CHAIN ANIONS; CIRCUMSTELLAR ENVELOPE; AGB STARS; INTERSTELLAR; MOLECULES; CHEMISTRY; IRC; EXCITATION; CLOUDS AB A new chemical model is presented for the carbon-rich circumstellar envelope (CSE) of the asymptotic giant branch star IRC+10216. The model includes shells of matter with densities that are enhanced relative to the surrounding circumstellar medium. The chemical model uses an updated reaction network including reactions from the RATE06 database and a more detailed anion chemistry. In particular, new mechanisms are considered for the formation of CN-, C3N-, and C2H-, and for the reactions of hydrocarbon anions with atomic nitrogen and with the most abundant cations in the CSE. New reactions involving H- are included which result in the production of significant amounts of C2H- and CN- in the inner envelope. The calculated radial molecular abundance profiles for the hydrocarbons C2H, C4H, and C6H and the cyanopolyynes HC3N and HC5N show narrow peaks which are in better agreement with observations than previous models. Thus, the narrow rings observed in molecular microwave emission surrounding IRC+10216 are interpreted as arising in regions of the envelope where the gas and dust densities are greater than the surrounding circumstellar medium. Our models show that CN- and C2H- may be detectable in IRC+10216 despite the very low theorized radiative electron attachment rates of their parent neutral species. We also show that magnesium isocyanide (MgNC) can be formed in the outer envelope through radiative association involving Mg+ and the cyanopolyyne species. C1 [Cordiner, M. A.; Millar, T. J.] Queens Univ Belfast, Astrophys Res Ctr, Sch Math & Phys, Belfast BT7 1NN, Antrim, North Ireland. RP Cordiner, MA (reprint author), NASA, Goddard Space Flight Ctr, Solar Syst Explorat Div, Mailstop 690-3, Greenbelt, MD 20771 USA. EM m.cordiner@qub.ac.uk OI Millar, Tom/0000-0001-5178-3656 FU QUB; STFC FX We gratefully acknowledge Veronica Bierbaum and Eric Herbst for their contributions to this work regarding the calculation of branching ratios for reactions between anions and nitrogen atoms. M.A.C. thanks QUB for financial support. Astrophysics at QUB is supported by a grant from the STFC. NR 48 TC 51 Z9 51 U1 0 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD MAY 20 PY 2009 VL 697 IS 1 BP 68 EP 78 DI 10.1088/0004-637X/697/1/68 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 441JB UT WOS:000265764000007 ER PT J AU Jewell, JB Eriksen, HK Wandelt, BD O'Dwyer, IJ Huey, G Gorski, KM AF Jewell, J. B. Eriksen, H. K. Wandelt, B. D. O'Dwyer, I. J. Huey, Greg Gorski, K. M. TI A MARKOV CHAIN MONTE CARLO ALGORITHM FOR ANALYSIS OF LOW SIGNAL-TO-NOISE COSMIC MICROWAVE BACKGROUND DATA SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmic microwave background; cosmology: observations; methods: numerical ID POWER SPECTRUM ESTIMATION; PROBE WMAP OBSERVATIONS; BAYESIAN-ANALYSIS; SKY MAPS AB We present a new Markov Chain Monte Carlo (MCMC) algorithm for cosmic microwave background (CMB) analysis in the low signal-to-noise regime. This method builds on and complements the previously described CMB Gibbs sampler, and effectively solves the low signal-to-noise inefficiency problem of the direct Gibbs sampler. The new algorithm is a simple Metropolis-Hastings sampler with a general proposal rule for the power spectrum, C(l), followed by a particular deterministic rescaling operation of the sky signal, s. The acceptance probability for this joint move depends on the sky map only through the difference of chi(2) between the original and proposed sky sample, which is close to unity in the low signal-to-noise regime. The algorithm is completed by alternating this move with a standard Gibbs move. Together, these two proposals constitute a computationally efficient algorithm for mapping out the full joint CMB posterior, both in the high and low signal-to-noise regimes. C1 [Jewell, J. B.; O'Dwyer, I. J.; Huey, Greg; Gorski, K. M.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Jewell, J. B.; Gorski, K. M.] CALTECH, Pasadena, CA 91125 USA. [Eriksen, H. K.] Univ Oslo, Inst Theoret Astrophys, N-0315 Oslo, Norway. [Eriksen, H. K.] Univ Oslo, Ctr Math Applicat, N-0316 Oslo, Norway. [Wandelt, B. D.] Univ Illinois, Dept Phys, Urbana, IL 61801 USA. [Wandelt, B. D.] Univ Illinois, Dept Astron, Urbana, IL 61801 USA. [Gorski, K. M.] Univ Warsaw Observ, PL-00478 Warsaw, Poland. RP Jewell, JB (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM Jeffrey.B.Jewell@jpl.nasa.gov; h.k.k.eriksen@astro.uio.no OI WANDELT, Benjamin/0000-0002-5854-8269 FU Research Council of Norway FX We acknowledge use of the HEALPix9 software (Gorski et al. 2005) and analysis package for deriving the results in this paper. H.K.E. acknowledges financial support from the Research Council of Norway. The research described in this paper was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. NR 25 TC 15 Z9 15 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAY 20 PY 2009 VL 697 IS 1 BP 258 EP 268 DI 10.1088/0004-637X/697/1/258 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 441JB UT WOS:000265764000022 ER PT J AU Bauschlicher, CW Peeters, E Allamandola, LJ AF Bauschlicher, Charles W., Jr. Peeters, Els Allamandola, Louis J. TI THE INFRARED SPECTRA OF VERY LARGE IRREGULAR POLYCYCLIC AROMATIC HYDROCARBONS (PAHs): OBSERVATIONAL PROBES OF ASTRONOMICAL PAH GEOMETRY, SIZE, AND CHARGE SO ASTROPHYSICAL JOURNAL LA English DT Article DE astrochemistry; infrared: ISM; ISM: lines and bands; ISM: molecules; line: identification; molecular data; techniques: spectroscopic ID INTERSTELLAR-EMISSION FEATURE; MIDINFRARED SPECTRA; REFLECTION NEBULAE; MICRON REGION; HII-REGIONS; BANDS; SPECTROSCOPY; MOLECULES; GALAXIES; FEATURES AB The mid-infrared (IR) spectra of six large, irregular polycyclic aromatic hydrocarbons (PAHs) with formulae (C(84)H(24)-C(120)H(36)) have been computed using density functional theory (DFT). Trends in the dominant band positions and intensities are compared to those of large, compact PAHs as a function of geometry, size, and charge. Irregular edge moieties that are common in terrestrial PAHs, such as bay regions and rings with quartet hydrogens, are shown to be uncommon in astronomical PAHs. As for all PAHs comprised solely of C and H reported to date, mid-IR emission from irregular PAHs fails to produce a strong CC(str) band at 6.2 mu m, the position characteristic of the important, class A astronomical PAH spectra. Earlier studies showed that inclusion of nitrogen within a PAH shifts this to 6.2 mu m for PAH cations. Here we show that this band shifts to 6.3 mu m in nitrogenated PAH anions, close to the position of the CC stretch in class B astronomical PAH spectra. Thus, nitrogenated PAHs may be important in all sources and the peak position of the CC stretch near 6.2 mu m appears to directly reflect the PAH cation to anion ratio. Large irregular PAHs exhibit features at 7.8 mu m but lack them near 8.6 mu m. Hence, the 7.7 mu m astronomical feature is produced by a mixture of small and large PAHs while the 8.6 mu m band can only be produced by large compact PAHs. As with the CC(str), the position and profile of these bands reflect the PAH cation to anion ratio. C1 [Bauschlicher, Charles W., Jr.; Allamandola, Louis J.] NASA, Ames Res Ctr, Space Technol Div, Moffett Field, CA 94035 USA. [Peeters, Els] Univ Western Ontario, Dept Phys & Astron, London, ON N6A 3K7, Canada. [Peeters, Els] SETI Inst, Mountain View, CA 94043 USA. RP Bauschlicher, CW (reprint author), NASA, Ames Res Ctr, Space Technol Div, Mail Stop 230-3, Moffett Field, CA 94035 USA. EM Charles.W.Bauschlicher@nasa.gov; epeeters@uwo.ca; Louis.J.Allamandola@nasa.gov FU NASA's; Spitzer Space Telescope Archival and General Observer Program FX We thank Doug Hudgins for fruitful, animated discussions and his insightful advice regarding Figure 13. We are particularly grateful to an anonymous referee for careful reading of the manuscript. We very gratefully acknowledge sustained support from NASA's Long Term Space Astrophysics and Astrobiology Programs, and the Spitzer Space Telescope Archival and General Observer Program. NR 56 TC 84 Z9 84 U1 0 U2 20 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAY 20 PY 2009 VL 697 IS 1 BP 311 EP 327 DI 10.1088/0004-637X/697/1/311 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 441JB UT WOS:000265764000028 ER PT J AU Dai, X Assef, RJ Kochanek, CS Brodwin, M Brown, MJI Caldwell, N Cool, RJ Dey, A Eisenhardt, P Eisenstein, D Gonzalez, AH Jannuzi, BT Jones, C Murray, SS Stern, D AF Dai, X. Assef, R. J. Kochanek, C. S. Brodwin, M. Brown, M. J. I. Caldwell, N. Cool, R. J. Dey, A. Eisenhardt, P. Eisenstein, D. Gonzalez, A. H. Jannuzi, B. T. Jones, C. Murray, S. S. Stern, D. TI MID-INFRARED GALAXY LUMINOSITY FUNCTIONS FROM THE AGN AND GALAXY EVOLUTION SURVEY SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: evolution; galaxies: luminosity function, mass function ID SPITZER-SPACE-TELESCOPE; STAR-FORMING GALAXIES; DIGITAL SKY SURVEY; ARRAY CAMERA IRAC; WIDE-FIELD SURVEY; VLT DEEP SURVEY; REDSHIFT SURVEY; RED SEQUENCE; DATA RELEASE; DENSITY AB We present galaxy luminosity functions at 3.6, 4.5, 5.8, and 8.0 mu m measured by combining photometry from the IRAC Shallow Survey with redshifts from the AGN and Galaxy Evolution Survey ( AGES) of the NOAO Deep Wide-Field Survey Bootes field. The well defined IRAC samples contain 3800-5800 galaxies for the 3.6-8.0 mu m bands with spectroscopic redshifts and z < 0.6. We obtained relatively complete luminosity functions in the local redshift bin of z < 0.2 for all four IRAC channels that are well fitted by Schechter functions. After analyzing the samples for the whole redshift range, we found significant evolution in the luminosity functions for all four IRAC channels that can be fitted as an evolution in M-* with redshift, Delta M-* = Qz. While we measured Q = 1.2 +/- 0.4 and 1.1 +/- 0.4 in the 3.6 and 4.5 mu m bands consistent with the predictions from a passively evolving population, we obtained Q = 1.8 +/- 1.1 in the 8.0 mu m band consistent with other evolving star formation rate estimates. We compared our luminosity functions with the predictions of semianalytical galaxy formation and found the best agreement at 3.6 and 4.5 mu m, rough agreement at 8.0 mu m, and a large mismatch at 5.8 mu m. These models also predicted a comparable Q-value to our luminosity functions at 8.0 mu m, but predicted smaller values at 3.6 and 4.5 mu m. We also measured the luminosity functions separately for early- and late-type galaxies. While the luminosity functions of late-type galaxies resemble those for the total population, the luminosity functions of early- type galaxies in the 3.6 and 4.5 mu m bands indicate deviations from the passive evolution model, especially from the measured flat luminosity density evolution. Combining our estimates with other measurements in the literature, we found 53 +/- 18% of the present stellar mass of early- type galaxies was assembled at z = 0.7. C1 [Dai, X.; Assef, R. J.; Kochanek, C. S.] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA. [Brodwin, M.; Dey, A.; Jannuzi, B. T.] Natl Opt Astron Observ, Tucson, AZ 85726 USA. [Brown, M. J. I.] Monash Univ, Sch Phys, Clayton, Vic 3800, Australia. [Caldwell, N.; Jones, C.; Murray, S. S.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Cool, R. J.; Eisenstein, D.] Univ Arizona, Steward Observ, Tucson, AZ 85121 USA. [Eisenhardt, P.; Stern, D.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Gonzalez, A. H.] Univ Florida, Dept Astron, Gainesville, FL 32611 USA. RP Dai, X (reprint author), Ohio State Univ, Dept Astron, 174 W 18Th Ave, Columbus, OH 43210 USA. EM xinyu@astronomy.ohio-state.edu RI Brown, Michael/B-1181-2015; Dai, Xinyu/B-5735-2011 OI Brown, Michael/0000-0002-1207-9137; Dai, Xinyu/0000-0001-9203-2808 NR 54 TC 21 Z9 21 U1 1 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD MAY 20 PY 2009 VL 697 IS 1 BP 506 EP 521 DI 10.1088/0004-637X/697/1/506 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 441JB UT WOS:000265764000042 ER PT J AU Collins, KA Grady, CA Hamaguchi, K Wisniewski, JP Brittain, S Sitko, M Carpenter, WJ Williams, JP Mathews, GS Williger, GM van Boekel, R Carmona, A Henning, T van den Ancker, ME Meeus, G Chen, XP Petre, R Woodgate, BE AF Collins, K. A. Grady, C. A. Hamaguchi, K. Wisniewski, J. P. Brittain, S. Sitko, M. Carpenter, W. J. Williams, J. P. Mathews, G. S. Williger, G. M. van Boekel, R. Carmona, A. Henning, Th. van den Ancker, M. E. Meeus, G. Chen, X. P. Petre, R. Woodgate, B. E. TI HD 100453: A LINK BETWEEN GAS-RICH PROTOPLANETARY DISKS AND GAS-POOR DEBRIS DISKS SO ASTROPHYSICAL JOURNAL LA English DT Review DE binaries: visual; planetary systems: protoplanetary disks; stars: individual (HD 100453, 51 Eri, AT Mic, HD 169142; 2MASSWJ1207334 393254); stars: low-mass, brown dwarfs; stars: pre-main sequence ID HERBIG-AE STAR; X-RAY-EMISSION; INTERMEDIATE-MASS STARS; MAIN-SEQUENCE STARS; TELESCOPE ADVANCED CAMERA; T-TAURI STARS; AE/BE STARS; CO EMISSION; YOUNG STARS; INFRARED SPECTROGRAPH AB HD 100453 has an IR spectral energy distribution (SED) which can be fit with a power law plus a blackbody. Previous analysis of the SED suggests that the system is a young Herbig Ae star with a gas-rich, flared disk. We reexamine the evolutionary state of the HD 100453 system by refining its age (based on a candidate low-mass companion) and by examining limits on the disk extent, mass accretion rate, and gas content of the disk environment. We confirm that HD 100453B is a common proper motion companion to HD 100453A, with a spectral type of M4.0V-M4.5V, and derive an age of 10 +/- 2 Myr. We find no evidence of mass accretion onto the star. Chandra ACIS-S imagery shows that the Herbig Ae star has L(x)/L(bol) and an X-ray spectrum similar to nonaccreting beta Pic Moving Group early F stars. Moreover, the disk lacks the conspicuous Fe II emission and excess FUV continuum seen in spectra of actively accreting Herbig Ae stars, and from the FUV continuum, we find the accretion rate is < 1.4 x 10(-9) M(circle dot) yr(-1). A sensitive upper limit to the CO J = 3-2 intensity indicates that the gas in the outer disk is likely optically thin. Assuming a [CO]/[H(2)] abundance of 1 x 10(-4) and a depletion factor of 10(3), we find that the mass of cold molecular gas is less than similar to 0.33 M(J) and that the gas-to-dust ratio is no more than similar to 4:1 in the outer disk. The combination of a high fractional IR excess luminosity, a relatively old age, an absence of accretion signatures, and an absence of detectable circumstellar molecular gas suggests that the HD 100453 system is in an unusual state of evolution between a gas-rich protoplanetary disk and a gas-poor debris disk. C1 [Collins, K. A.; Williger, G. M.] Univ Louisville, Dept Phys & Astron, Louisville, KY 40292 USA. [Grady, C. A.] Eureka Sci, Oakland, CA 96002 USA. [Grady, C. A.] GSFC, Oakland, CA 96002 USA. [Hamaguchi, K.] NASA, Goddard Space Flight Ctr, CRESST, Greenbelt, MD 20771 USA. [Hamaguchi, K.] NASA, Goddard Space Flight Ctr, Xray Astrophys Lab, Greenbelt, MD 20771 USA. [Hamaguchi, K.] Univ Maryland, Dept Phys, Baltimore, MD 21250 USA. [Wisniewski, J. P.] Univ Washington, Dept Astron, Seattle, WA 98195 USA. [Brittain, S.] Clemson Univ, Clemson, SC 29634 USA. [Sitko, M.] Univ Cincinnati, Space Sci Inst, Cincinnati, OH 45221 USA. [Mathews, G. S.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. [Williger, G. M.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Williger, G. M.] Catholic Univ, Dept Phys, Washington, DC 20064 USA. [van Boekel, R.; Carmona, A.; Henning, Th.; Chen, X. P.] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Carmona, A.] Univ Geneva, Observ Geneva, CH-1290 Versoix, Switzerland. [Carmona, A.] ISDC Ch Ecogia 16, CH-1290 Versoix, Switzerland. [Carmona, A.; van den Ancker, M. E.] European So Observ, D-85748 Garching, Germany. [Meeus, G.] AIP, D-14482 Potsdam, Germany. RP Collins, KA (reprint author), Univ Louisville, Dept Phys & Astron, Louisville, KY 40292 USA. EM karen.collins@insightbb.com; Carol.A.Grady@nasa.gov; Kenji.Hamaguchi@nasa.gov; wisniewski@astro.washington.edu; sbritt@clemson.edu; Michael.Sitko@uc.edu; wcarpenter4@cinci.rr.com; jpw@ifa.hawaii.edu; gmathews@ifa.hawaii.edu; williger@physics.louisville.edu; boekel@mpia-hd.mpg.de; andres.carmona@unige.ch; henning@mpia-hd.mpg.de; mvandena@eso.org; gwen@aip.de; chen@mpia-hd.mpg.de; petre@lheavx.gsfc.nasa.gov; Bruce.E.Woodgate@nasa.gov RI Woodgate, Bruce/D-2970-2012; Brittain, Sean/K-9001-2012; OI Brittain, Sean/0000-0001-5638-1330; Williams, Jonathan/0000-0001-5058-695X NR 106 TC 19 Z9 19 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAY 20 PY 2009 VL 697 IS 1 BP 557 EP 572 DI 10.1088/0004-637X/697/1/557 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 441JB UT WOS:000265764000046 ER PT J AU Guieu, S Rebull, LM Stauffer, JR Hillenbrand, LA Carpenter, JM Noriega-Crespo, A Padgett, DL Cole, DM Carey, SJ Stapelfeldt, KR Strom, SE AF Guieu, S. Rebull, L. M. Stauffer, J. R. Hillenbrand, L. A. Carpenter, J. M. Noriega-Crespo, A. Padgett, D. L. Cole, D. M. Carey, S. J. Stapelfeldt, K. R. Strom, S. E. TI THE NORTH AMERICAN AND PELICAN NEBULAE. I. IRAC OBSERVATIONS SO ASTROPHYSICAL JOURNAL LA English DT Article DE circumstellar matter; infrared: ISM; infrared: stars; ISM: clouds; ISM: individual (NGC 7000, IC 5070); stars: formation; stars: pre-main sequence ID SPITZER C2D SURVEY; INTERSTELLAR CLOUDS; MOLECULAR CLOUDS; SPACE-TELESCOPE; MASS STARS; NEARBY; CLUSTER; JETS; SIMULATIONS; EXTINCTION AB We present a 9 deg(2) map of the North American and Pelican Nebulae regions obtained in all four Infrared Array Camera (IRAC) channels with the Spitzer Space Telescope. The resulting photometry is merged with that at JHK(s) from Two Micron All Sky Survey and a more spatially limited BVI survey from previous ground-based work. We use a mixture of color-color diagrams to select a minimally contaminated set of more than 1600 objects that we claim are young stellar objects (YSOs) associated with the star-forming region. Because our selection technique uses infrared excess as a requirement, our sample is strongly biased against inclusion of Class III YSOs. The distribution of IRAC spectral slopes for our YSOs indicates that most of these objects are Class II, with a peak toward steeper spectral slopes but a substantial contribution from a tail of Flat spectrum and Class I type objects. By studying the small fraction of the sample that is optically visible, we infer a typical age of a few Myr for the low-mass population. The young stars are clustered, with about a third of them located in eight clusters that are located within or near the LDN 935 dark cloud. Half of the YSOs are located in regions with surface densities higher than 1000 YSOs/deg(2). The Class I objects are more clustered than the Class II stars. C1 [Guieu, S.; Rebull, L. M.; Stauffer, J. R.; Noriega-Crespo, A.; Padgett, D. L.; Carey, S. J.] CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA. [Hillenbrand, L. A.; Carpenter, J. M.] CALTECH, Dept Astron, Pasadena, CA 91125 USA. [Cole, D. M.; Stapelfeldt, K. R.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Strom, S. E.] Natl Opt Astron Observ, Tucson, AZ USA. RP Guieu, S (reprint author), CALTECH, Spitzer Sci Ctr, M-S 220-6,1200 E Calif Blvd, Pasadena, CA 91125 USA. EM guieu@ipac.caltech.edu RI Stapelfeldt, Karl/D-2721-2012; OI Rebull, Luisa/0000-0001-6381-515X FU National Aeronautics and Space Administration FX The research described in this paper was partially carried out at the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. NR 39 TC 23 Z9 23 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAY 20 PY 2009 VL 697 IS 1 BP 787 EP 800 DI 10.1088/0004-637X/697/1/787 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 441JB UT WOS:000265764000066 ER PT J AU Madzunkov, SM MacAskill, JA Chutjian, A Ehrenfreund, P Darrach, MR Vidali, G Shortt, BJ AF Madzunkov, S. M. MacAskill, J. A. Chutjian, A. Ehrenfreund, P. Darrach, M. R. Vidali, G. Shortt, B. J. TI FORMATION OF FORMALDEHYDE AND CARBON DIOXIDE ON AN ICY GRAIN ANALOG USING FAST HYDROGEN ATOMS SO ASTROPHYSICAL JOURNAL LA English DT Article DE astrochemistry; circumstellar matter; ISM: molecules; stars: winds, outflows ID H2O-CO ICE; SOLID CO; 10 K; MOLECULES; CHEMISTRY; METHANOL; SURFACE; GAS; DESORPTION; WATER AB Formaldehyde (H(2)CO) and carbon dioxide (CO(2)) were produced in collisions of a superthermal, 3 eV beam of H((2)S) atoms with CO molecules adsorbed on a gold surface at 4.8 K. The reaction-generated products were detected and analyzed using the techniques of temperature programmed desorption (TPD), quadrupole mass spectrometry, and a novel application of the Metropolis algorithm, random-walk procedure to identify the unique fractionation patterns of H(2)CO and CO(2) from the patterns of other species such as N(2), CO, and H(2)O embedded in the CO blanket and devolved in the TPD/mass spectrometry process. Reaction sequences are given to account for the formation of H(2)CO and CO(2). C1 [Madzunkov, S. M.; MacAskill, J. A.; Chutjian, A.; Darrach, M. R.] CALTECH, Jet Prop Lab, Atom & Mol Phys Grp, Pasadena, CA 91109 USA. [Ehrenfreund, P.] Leiden Inst Chem, NL-2300 RA Leiden, Netherlands. [Vidali, G.] Syracuse Univ, Dept Phys, Syracuse, NY 13244 USA. RP Madzunkov, SM (reprint author), CALTECH, Jet Prop Lab, Atom & Mol Phys Grp, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. FU National Aeronautics and Space Administration through California Institute of Technology FX Helpful discussions with A. Glassgold, M. Gudipati, M. Mumma, and J. Nuth are gratefully acknowledged. This work was carried out at JPL/Caltech, and was supported by the National Aeronautics and Space Administration through agreement with the California Institute of Technology. NR 35 TC 8 Z9 8 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAY 20 PY 2009 VL 697 IS 1 BP 801 EP 806 DI 10.1088/0004-637X/697/1/801 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 441JB UT WOS:000265764000067 ER PT J AU Allers, KN Liu, MC Shkolnik, E Cushing, MC Dupuy, TJ Mathews, GS Reid, IN Cruz, KL Vacca, WD AF Allers, K. N. Liu, Michael C. Shkolnik, Evgenya Cushing, Michael C. Dupuy, Trent J. Mathews, Geoffrey S. Reid, I. Neill Cruz, Kelle L. Vacca, W. D. TI 2MASS 22344161+4041387AB: A WIDE, YOUNG, ACCRETING, LOW-MASS BINARY IN THE LkH alpha 233 GROUP SO ASTROPHYSICAL JOURNAL LA English DT Article DE binaries: visual; infrared: stars; stars: formation; stars: low-mass, brown dwarfs ID STAR ADAPTIVE OPTICS; T-TAURI STARS; SCORPIUS OB ASSOCIATION; NEAR-INFRARED SPECTRA; BROWN DWARFS; HYDRAE ASSOCIATION; FORMING REGION; CIRCUMSTELLAR DISKS; EVOLUTIONARY MODELS; SOLAR NEIGHBORHOOD AB We report the discovery of a young, 0 ''.16 binary, 2M2234+4041AB, found as the result of a Keck laser guide star adaptive optics imaging survey of young field ultracool dwarfs. Spatially resolved near-infrared photometry and spectroscopy indicate that the luminosity and temperature ratios of the system are near unity. From optical and near-infrared spectroscopy, we determine a composite spectral type of M6 for the system. Gravity-sensitive spectral features in the spectra of 2M2234+4041AB are best matched to those of young objects (similar to 1 Myr old). A comparison of the T(eff) and age of 2M2234+4041AB to evolutionary models indicates that the mass of each component is 0.10(-0.04)(+0.075) M(circle dot). Emission lines of H alpha in the composite optical spectrum of the system and Br gamma in spatially resolved near-IR spectra of the two components indicate that the system is actively accreting. Both components of the system have IR excesses, indicating that they both harbor circumstellar disks. Though 2M2234+4041AB was originally identified as a young field dwarf, it lies 1'.5 from the well-studied Herbig Ae/Be star, LkH alpha 233. The distance to LkH alpha 233 is typically assumed to be 880 pc. It is unlikely that 2M2234+4041AB could be this distant, as it would then be more luminous than any known Taurus objects of similar spectral type. We re-evaluate the distance to the LkH alpha 233 group and find a value of 325(-50)(+72) pc, based on the Hipparcos distance to a nearby B3-type group member (HD 213976). 2M2234+4041AB is the first low-mass star to be potentially associated with the LkH alpha 233 group. At a distance of 325 pc, its projected physical separation is 51 AU, making it one of the growing number of wide, low-mass binaries found in young star-forming regions. C1 [Allers, K. N.; Liu, Michael C.; Cushing, Michael C.; Dupuy, Trent J.; Mathews, Geoffrey S.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. [Shkolnik, Evgenya] Carnegie Inst Washington, Dept Terr Magnetism, Washington, DC 20015 USA. [Reid, I. Neill] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Cruz, Kelle L.] CALTECH, Dept Astron, Pasadena, CA 91125 USA. [Vacca, W. D.] NASA, Ames Res Ctr, SOFIA USRA, Moffett Field, CA 94035 USA. RP Allers, KN (reprint author), Univ Hawaii, Inst Astron, 2680 Woodlawn Dr, Honolulu, HI 96822 USA. FU NSF [AST-0507833, AST-0407441]; Alfred P. Sloan Research Fellowship; NASA/GALEX [NNX07AJ43G]; NASA Origins of Solar Systems [NNX07AI83G]; Space Telescope Science Institute [10879]; NASA [NAS 5-26555] FX We gratefully acknowledge the Keck LGS AO team for their exceptional efforts in bringing the LGS AO system to fruition. It is a pleasure to thank Randy Campbell, Jim Lyke, Al Conrad, Hien Tran, Christine Melcher, Cindy Wilburn, Joel Aycock, Jason McElroy, and the Keck Observatory staff for assistance with the observations. This work is based in part on data products produced at the TERAPIX data center located at the Institut d'Astrophysique de Paris. We also thank John Rayner and the IRTF Observatory staff for assistance with our SpeX observations and data reduction. We are appreciative of conversations with George Herbig on the origin of 2M2234+4041AB and the nature of other nearby young stars. We also thank Jeffrey Rich for translating Chernyshev & Shevchenko (1988) into English. The authors sincerely thank Roy Gal for providing Tek/UH88 '' imaging of 2M2234+4041AB. We are grateful to Dan Jaffe, Casey Deen, Jasmina Marsh, and Alan Tokunaga for providing the near-infrared spectrum of TWA8B. This research has benefited from the M, L, and T dwarf compendium housed at DwarfArchives.org and maintained by Chris Gelino, Davy Kirkpatrick, and Adam Burgasser. KLC is supported by NASA through the Spitzer Space Telescope Fellowship Program, through a contract issued by the Jet Propulsion Laboratory, California Institute of Technology under a contract with National Aeronautics and Space Administration. M. C. L., K. N. A., and T. J. D. acknowledge support for this work from NSF grants AST-0507833 and AST-0407441. M. C. L. also acknowledges support from an Alfred P. Sloan Research Fellowship. E. S. acknowledges support from NASA/GALEX grant NNX07AJ43G. K. N. A. was partially supported by NASA Origins of Solar Systems grant NNX07AI83G. This work was partially supported by NASA through a grant associated with HST program 10879 from the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5-26555. NR 100 TC 28 Z9 28 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAY 20 PY 2009 VL 697 IS 1 BP 824 EP 835 DI 10.1088/0004-637X/697/1/824 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 441JB UT WOS:000265764000069 ER PT J AU Abdo, AA Ackermann, M Atwood, WB Axelsson, M Baldini, L Ballet, J Barbiellini, G Bastieri, D Baughman, BM Bechtol, K Bellazzini, R Berenji, B Blandford, RD Bloom, ED Bogaert, G Bonamente, E Borgland, AW Bregeon, J Brez, A Brigida, M Bruel, P Burnett, TH Caliandro, GA Cameron, RA Caraveo, PA Casandjian, JM Cavazzuti, E Cecchi, C Charles, E Chekhtman, A Cheung, CC Chiang, J Ciprini, S Claus, R Cohen-Tanugi, J Colafrancesco, S Conrad, J Costamante, L Cutini, S Dermer, CD de Angelis, A de Palma, F Digel, SW Silva, EDE Drell, PS Dubois, R Dumora, D Edmonds, Y Farnier, C Favuzzi, C Ferrara, EC Fleury, P Focke, WB Foschini, L Frailis, M Fuhrmann, L Fukazawa, Y Funk, S Fusco, P Gargano, F Gasparrini, D Gehrels, N Germani, S Giebels, B Giglietto, N Giordano, F Giroletti, M Glanzman, T Godfrey, G Grenier, IA Grondin, MH Grove, JE Guillemot, L Guiriec, S Harding, AK Hartman, RC Hayashida, M Hays, E Healey, SE Hughes, RE Johannesson, G Johnson, AS Johnson, RP Johnson, WN Kadler, M Kamae, T Katagiri, H Kataoka, J Kawai, N Kerr, M Knodlseder, J Kocian, ML Kuehn, F Kuss, M Latronico, L Lee, SH Lemoine-Goumard, M Longo, F Loparco, F Lott, B Lovellette, MN Lubrano, P Madejski, GM Makeev, A Marelli, M Mazziotta, MN McEnery, JE McGlynn, S Meurer, C Michelson, PF Mitthumsiri, W Mizuno, T Moiseev, AA Monte, C Monzani, ME Morselli, A Moskalenko, IV Murgia, S Nolan, PL Nuss, E Ohno, M Ohsugi, T Ojha, R Omodei, N Orlando, E Ormes, JF Paneque, D Panetta, JH Parent, D Pepe, M Pesce-Rollins, M Piron, F Porter, TA Raino, S Rando, R Razzano, M Reimer, A Reimer, O Reposeur, T Reyes, LC Ritz, S Rochester, LS Rodriguez, AY Romani, RW Roth, M Ryde, F Sadrozinski, HFW Sambruna, R Sanchez, D Sander, A Parkinson, PMS Sgro, C Shaw, MS Siskind, EJ Smith, DA Smith, PD Spandre, G Spinelli, P Starck, JL Strickman, MS Suson, DJ Tajima, H Takahashi, H Tanaka, T Thayer, JB Thayer, JG Thompson, DJ Tibaldo, L Tibolla, O Torres, DF Tosti, G Tramacere, A Usher, TL Vilchez, N Vitale, V Waite, AP Wang, P Winer, BL Wood, KS Ylinen, T Ziegler, M Edwards, PG Chester, MM Burrows, DN Hauser, M Wagner, S AF Abdo, A. A. Ackermann, M. Atwood, W. B. Axelsson, M. Baldini, L. Ballet, J. Barbiellini, G. Bastieri, D. Baughman, B. M. Bechtol, K. Bellazzini, R. Berenji, B. Blandford, R. D. Bloom, E. D. Bogaert, G. Bonamente, E. Borgland, A. W. Bregeon, J. Brez, A. Brigida, M. Bruel, P. Burnett, T. H. Caliandro, G. A. Cameron, R. A. Caraveo, P. A. Casandjian, J. M. Cavazzuti, E. Cecchi, C. Charles, E. Chekhtman, A. Cheung, C. C. Chiang, J. Ciprini, S. Claus, R. Cohen-Tanugi, J. Colafrancesco, S. Conrad, J. Costamante, L. Cutini, S. Dermer, C. D. de Angelis, A. de Palma, F. Digel, S. W. do Couto E Silva, E. Drell, P. S. Dubois, R. Dumora, D. Edmonds, Y. Farnier, C. Favuzzi, C. Ferrara, E. C. Fleury, P. Focke, W. B. Foschini, L. Frailis, M. Fuhrmann, L. Fukazawa, Y. Funk, S. Fusco, P. Gargano, F. Gasparrini, D. Gehrels, N. Germani, S. Giebels, B. Giglietto, N. Giordano, F. Giroletti, M. Glanzman, T. Godfrey, G. Grenier, I. A. Grondin, M. -H. Grove, J. E. Guillemot, L. Guiriec, S. Harding, A. K. Hartman, R. C. Hayashida, M. Hays, E. Healey, S. E. Hughes, R. E. Johannesson, G. Johnson, A. S. Johnson, R. P. Johnson, W. N. Kadler, M. Kamae, T. Katagiri, H. Kataoka, J. Kawai, N. Kerr, M. Knoedlseder, J. Kocian, M. L. Kuehn, F. Kuss, M. Latronico, L. Lee, S. -H. Lemoine-Goumard, M. Longo, F. Loparco, F. Lott, B. Lovellette, M. N. Lubrano, P. Madejski, G. M. Makeev, A. Marelli, M. Mazziotta, M. N. McEnery, J. E. McGlynn, S. Meurer, C. Michelson, P. F. Mitthumsiri, W. Mizuno, T. Moiseev, A. A. Monte, C. Monzani, M. E. Morselli, A. Moskalenko, I. V. Murgia, S. Nolan, P. L. Nuss, E. Ohno, M. Ohsugi, T. Ojha, R. Omodei, N. Orlando, E. Ormes, J. F. Paneque, D. Panetta, J. H. Parent, D. Pepe, M. Pesce-Rollins, M. Piron, F. Porter, T. A. Raino, S. Rando, R. Razzano, M. Reimer, A. Reimer, O. Reposeur, T. Reyes, L. C. Ritz, S. Rochester, L. S. Rodriguez, A. Y. Romani, R. W. Roth, M. Ryde, F. Sadrozinski, H. F. -W. Sambruna, R. Sanchez, D. Sander, A. Parkinson, P. M. Saz Sgro, C. Shaw, M. S. Siskind, E. J. Smith, D. A. Smith, P. D. Spandre, G. Spinelli, P. Starck, J. -L. Strickman, M. S. Suson, D. J. Tajima, H. Takahashi, H. Tanaka, T. Thayer, J. B. Thayer, J. G. Thompson, D. J. Tibaldo, L. Tibolla, O. Torres, D. F. Tosti, G. Tramacere, A. Usher, T. L. Vilchez, N. Vitale, V. Waite, A. P. Wang, P. Winer, B. L. Wood, K. S. Ylinen, T. Ziegler, M. Edwards, P. G. Chester, M. M. Burrows, D. N. Hauser, M. Wagner, S. CA Fermi LAT Collaboration TI FERMI/LARGE AREA TELESCOPE DISCOVERY OF GAMMA-RAY EMISSION FROM THE FLAT-SPECTRUM RADIO QUASAR PKS 1454-354 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: active; gamma rays: observations; quasars: individual (PKS 1454-354) ID SOURCE CATALOG; EGRET SOURCES; SKY SURVEY; IDENTIFICATIONS; SAMPLE; DISTRIBUTIONS; SOFTWARE; BLAZARS; MISSION; MODEL AB We report the discovery by the Large Area Telescope (LAT) onboard the Fermi Gamma-Ray Space Telescope of high-energy gamma-ray (GeV) emission from the flat-spectrum radio quasar PKS 1454-354 (z = 1.424). On 2008 September 4, the source rose to a peak flux of (3.5 +/- 0.7) x 10(-6) ph cm(-2) s(-1) (E > 100 MeV) on a timescale of hours and then slowly dropped over the following 2 days. No significant spectral changes occurred during the flare. Fermi/LAT observations also showed that PKS 1454-354 is the most probable counterpart of the unidentified EGRET source 3EG J1500-3509. Multiwavelength measurements performed during the following days (7 September with Swift; 6-7 September with the ground-based optical telescope Automated Telescope for Optical Monitoring; 13 September with the Australia Telescope Compact Array) resulted in radio, optical, UV, and X-ray fluxes greater than archival data, confirming the activity of PKS 1454-354. C1 [Foschini, L.] Osserv Astron Brera, INAF, I-23807 Merate, LC, Italy. [Abdo, A. A.; Chekhtman, A.; Dermer, C. D.; Grove, J. E.; Johnson, W. N.; Lovellette, M. N.; Makeev, A.; Strickman, M. S.; Wood, K. S.] USN, Res Lab, Div Space Sci, Washington, DC 20375 USA. [Ackermann, M.; Bechtol, K.; Berenji, B.; Blandford, R. D.; Bloom, E. D.; Borgland, A. W.; Cameron, R. A.; Charles, E.; Chiang, J.; Claus, R.; Costamante, L.; Digel, S. W.; do Couto E Silva, E.; Drell, P. S.; Dubois, R.; Edmonds, Y.; Focke, W. B.; Funk, S.; Glanzman, T.; Godfrey, G.; Hayashida, M.; Healey, S. E.; Johannesson, G.; Johnson, A. S.; Kamae, T.; Kocian, M. L.; Lee, S. -H.; Madejski, G. M.; Michelson, P. F.; Mitthumsiri, W.; Monzani, M. E.; Moskalenko, I. V.; Murgia, S.; Nolan, P. L.; Paneque, D.; Reimer, A.; Reimer, O.; Rochester, L. S.; Romani, R. W.; Shaw, M. S.; Tajima, H.; Tanaka, T.; Thayer, J. B.; Thayer, J. G.; Tramacere, A.; Usher, T. L.; Waite, A. P.; Wang, P.] Stanford Univ, WW Hansen Expt Phys Lab, Kavli Inst Particle Astrophys & Cosmol, Dept Phys, Stanford, CA 94305 USA. [Ackermann, M.; Bechtol, K.; Berenji, B.; Blandford, R. D.; Bloom, E. D.; Borgland, A. W.; Cameron, R. A.; Charles, E.; Chiang, J.; Claus, R.; Costamante, L.; Digel, S. W.; do Couto E Silva, E.; Drell, P. S.; Dubois, R.; Edmonds, Y.; Focke, W. B.; Funk, S.; Glanzman, T.; Godfrey, G.; Hayashida, M.; Healey, S. E.; Johannesson, G.; Johnson, A. S.; Kamae, T.; Kocian, M. L.; Lee, S. -H.; Madejski, G. M.; Michelson, P. F.; Mitthumsiri, W.; Monzani, M. E.; Moskalenko, I. V.; Murgia, S.; Nolan, P. L.; Paneque, D.; Reimer, A.; Reimer, O.; Rochester, L. S.; Romani, R. W.; Shaw, M. S.; Tajima, H.; Tanaka, T.; Thayer, J. B.; Thayer, J. G.; Tramacere, A.; Usher, T. L.; Waite, A. P.; Wang, P.] Stanford Univ, SLAC Natl Lab, Stanford, CA 94305 USA. [Atwood, W. B.; Johnson, R. P.; Porter, T. A.; Sadrozinski, H. F. -W.; Parkinson, P. M. Saz; Ziegler, M.] Univ Calif Santa Cruz, Santa Cruz Inst Particle Phys, Dept Phys, Santa Cruz, CA 95064 USA. [Atwood, W. B.; Johnson, R. P.; Porter, T. A.; Sadrozinski, H. F. -W.; Parkinson, P. M. Saz; Ziegler, M.] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA. [Axelsson, M.; Brez, A.; Conrad, J.; McGlynn, S.; Meurer, C.; Ryde, F.; Ylinen, T.] Oskar Klein Ctr Cosmo Particle Phys, SE-10691 Stockholm, Sweden. [Axelsson, M.] Stockholm Univ, Dept Astron, SE-10691 Stockholm, Sweden. [Baldini, L.; Bellazzini, R.; Bregeon, J.; Brez, A.; Kuss, M.; Latronico, L.; Razzano, M.; Ryde, F.; Sgro, C.] Ist Nazl Fis Nucl, Sez Pisa, I-56127 Pisa, Italy. [Ballet, J.; Casandjian, J. M.; Grenier, I. A.; Starck, J. -L.] Univ Paris Diderot, CNRS, Serv Astrophys, Lab AIM,CEA,IRFU,CEA Saclay, F-91191 Gif Sur Yvette, France. [Barbiellini, G.; Longo, F.] Ist Nazl Fis Nucl, Sez Trieste, I-34127 Trieste, Italy. [Barbiellini, G.; Longo, F.] Univ Trieste, Dipartimento Fis, I-34127 Trieste, Italy. [Bastieri, D.; Rando, R.; Tibaldo, L.] Ist Nazl Fis Nucl, Sez Padova, I-35131 Padua, Italy. [Bastieri, D.; Rando, R.; Tibaldo, L.] Univ Padua, Dipartimento Fis G Galilei, I-35131 Padua, Italy. [Baughman, B. M.; Hughes, R. E.; Kuehn, F.; Sander, A.; Smith, P. D.; Winer, B. L.] Ohio State Univ, Dept Phys, Ctr Cosmol & Astroparticle Phys, Columbus, OH 43210 USA. [Bogaert, G.; Bruel, P.; Fleury, P.; Giebels, B.; Sanchez, D.] Ecole Polytech, CNRS, IN2P3, Lab Leprince Ringuet, F-91128 Palaiseau, France. [Bonamente, E.; Cecchi, C.; Ciprini, S.; Germani, S.; Lubrano, P.; Pepe, M.; Tosti, G.] Ist Nazl Fis Nucl, Sez Perugia, I-06123 Perugia, Italy. [Bonamente, E.; Cecchi, C.; Ciprini, S.; Germani, S.; Lubrano, P.; Pepe, M.; Tosti, G.] Univ Perugia, Dipartimento Fis, I-06123 Perugia, Italy. [Brigida, M.; Caliandro, G. A.; de Palma, F.; Favuzzi, C.; Fusco, P.; Giglietto, N.; Giordano, F.; Loparco, F.; Monte, C.; Raino, S.; Spinelli, P.] Univ Politecn Bari, Dipartimento Fis M Merlin, I-70126 Bari, Italy. [Brigida, M.; Caliandro, G. A.; de Palma, F.; Favuzzi, C.; Fusco, P.; Gargano, F.; Giglietto, N.; Giordano, F.; Loparco, F.; Mazziotta, M. N.; Monte, C.; Raino, S.; Spinelli, P.] Ist Nazl Fis Nucl, Sez Bari, I-70126 Bari, Italy. [Burnett, T. H.; Kerr, M.; Roth, M.] Univ Washington, Dept Phys, Seattle, WA 98195 USA. [Caraveo, P. A.; Marelli, M.] Ist Astrofis Spaziale & Fis Cosm, INAF, I-20133 Milan, Italy. [Cavazzuti, E.; Colafrancesco, S.; Cutini, S.; Gasparrini, D.] Agenzia Spaziale Italiana ASI Sci Data Ctr, I-00044 Frascati, Rome, Italy. [Chekhtman, A.] George Mason Univ, Fairfax, VA 22030 USA. [Kadler, M.; Moiseev, A. A.] NASA, Goddard Space Flight Ctr, CRESST, Greenbelt, MD 20771 USA. [Cohen-Tanugi, J.; Farnier, C.; Guiriec, S.; Nuss, E.; Piron, F.] Univ Montpellier 2, CNRS, IN2P3, Lab Phys Theor & Astroparticules, Montpellier, France. [Conrad, J.; McGlynn, S.; Ryde, F.; Ylinen, T.] Royal Inst Technol KTH, Dept Phys, SE-10691 Stockholm, Sweden. [Conrad, J.; Meurer, C.] Stockholm Univ, Dept Phys, SE-10691 Stockholm, Sweden. [de Angelis, A.; Frailis, M.] Univ Udine, Dipartimento Fis, I-33100 Udine, Italy. [de Angelis, A.; Frailis, M.] Grp Coll Udine, Ist Nazl Fis Nucl, Sez Trieste, I-33100 Udine, Italy. [Dumora, D.; Grondin, M. -H.; Guillemot, L.; Lemoine-Goumard, M.; Lott, B.; Parent, D.; Reposeur, T.; Smith, D. A.] Ctr Etud Nucl Bordeaux Gradignan, CNRS, IN2P3, UMR 5797, F-33175 Gradignan, France. [Dumora, D.; Grondin, M. -H.; Guillemot, L.; Lemoine-Goumard, M.; Lott, B.; Parent, D.; Reposeur, T.; Smith, D. A.] Univ Bordeaux, Ctr Etud Nucl Bordeaux Gradignan, UMR 5797, F-33175 Gradignan, France. [Fuhrmann, L.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Fukazawa, Y.; Katagiri, H.; Mizuno, T.; Ohsugi, T.; Takahashi, H.] Hiroshima Univ, Dept Phys Sci, Hiroshima 7398526, Japan. [Gehrels, N.; Ritz, S.] Univ Maryland, College Pk, MD 20742 USA. [Giroletti, M.] Inst Radioastron, INAF, I-40129 Bologna, Italy. [Kadler, M.] Dr Remeis Sternwarte Bamberg, D-96049 Bamberg, Germany. [Kadler, M.] Erlangen Ctr Astroparticle Phys, D-91058 Erlangen, Germany. [Kadler, M.] Univ Space Res Assoc, Columbia, MD 21044 USA. [Kataoka, J.] Waseda Univ, Shinjuku Ku, Tokyo 1698050, Japan. [Kawai, N.] RIKEN, Inst Phys & Chem Res, Cosm Radiat Lab, Wako, Saitama 3510198, Japan. [Kawai, N.] Tokyo Inst Technol, Dept Phys, Meguro, Tokyo 1528551, Japan. [Knoedlseder, J.; Vilchez, N.] CNRS UPS, Ctr Etud Spatiale Rayonnements, F-31028 Toulouse 4, France. [Morselli, A.; Vitale, V.] Ist Nazl Fis Nucl, Sez Roma Tor Vergata, I-00133 Rome, Italy. [Ohno, M.] JAXA, Inst Space & Astronaut Sci, Sagamihara, Kanagawa 2298510, Japan. [Ojha, R.] USN Observ, Washington, DC 20392 USA. [Orlando, E.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Ormes, J. F.] Univ Denver, Dept Phys & Astron, Denver, CO 80208 USA. [Reyes, L. C.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA. [Rodriguez, A. Y.; Torres, D. F.] CSIC, IEEC, Inst Ciencies Espai, Barcelona 08193, Spain. [Siskind, E. J.] NYCB Real Time Comp Inc, Lattingtown, NY 11560 USA. [Suson, D. J.] Purdue Univ Calumet, Dept Chem & Phys, Hammond, IN 46323 USA. [Tibolla, O.] Max Planck Inst Kernphys, D-69029 Heidelberg, Germany. [Torres, D. F.] ICREA, Barcelona, Spain. [Tramacere, A.] CIFS, I-10133 Turin, Italy. [Vitale, V.] Univ Roma Tor Vergata, Dipartimento Fis, I-10133 Turin, Italy. [Ylinen, T.] Univ Kalmar, Sch Pure & Appl Nat Sci, SE-39182 Kalmar, Sweden. [Edwards, P. G.] Paul Wild Observ, CSIRO, ATNF, Narrabri, NSW 2390, Australia. [Chester, M. M.; Burrows, D. N.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Hauser, M.; Wagner, S.] Heidelberg Univ, D-69117 Heidelberg, Germany. RP Foschini, L (reprint author), Osserv Astron Brera, INAF, I-23807 Merate, LC, Italy. EM luigi.foschini@brera.inaf.it RI Rando, Riccardo/M-7179-2013; Hays, Elizabeth/D-3257-2012; Johnson, Neil/G-3309-2014; Reimer, Olaf/A-3117-2013; Funk, Stefan/B-7629-2015; Gargano, Fabio/O-8934-2015; Loparco, Francesco/O-8847-2015; Johannesson, Gudlaugur/O-8741-2015; Moskalenko, Igor/A-1301-2007; Mazziotta, Mario /O-8867-2015; Sgro, Carmelo/K-3395-2016; Torres, Diego/O-9422-2016; Orlando, E/R-5594-2016; Tosti, Gino/E-9976-2013; De Angelis, Alessandro/B-5372-2009; Starck, Jean-Luc/D-9467-2011; Thompson, David/D-2939-2012; Harding, Alice/D-3160-2012; Gehrels, Neil/D-2971-2012; McEnery, Julie/D-6612-2012; Baldini, Luca/E-5396-2012; lubrano, pasquale/F-7269-2012; Morselli, Aldo/G-6769-2011; Foschini, Luigi/H-3833-2012; Nolan, Patrick/A-5582-2009; Kuss, Michael/H-8959-2012; giglietto, nicola/I-8951-2012 OI Marelli, Martino/0000-0002-8017-0338; Kadler, Matthias/0000-0001-5606-6154; Cutini, Sara/0000-0002-1271-2924; Berenji, Bijan/0000-0002-4551-772X; Gasparrini, Dario/0000-0002-5064-9495; Tramacere, Andrea/0000-0002-8186-3793; Baldini, Luca/0000-0002-9785-7726; Sgro', Carmelo/0000-0001-5676-6214; Giordano, Francesco/0000-0002-8651-2394; De Angelis, Alessandro/0000-0002-3288-2517; Frailis, Marco/0000-0002-7400-2135; Caraveo, Patrizia/0000-0003-2478-8018; Bastieri, Denis/0000-0002-6954-8862; Omodei, Nicola/0000-0002-5448-7577; Pesce-Rollins, Melissa/0000-0003-1790-8018; Axelsson, Magnus/0000-0003-4378-8785; Giroletti, Marcello/0000-0002-8657-8852; Reimer, Olaf/0000-0001-6953-1385; Funk, Stefan/0000-0002-2012-0080; Gargano, Fabio/0000-0002-5055-6395; Loparco, Francesco/0000-0002-1173-5673; Johannesson, Gudlaugur/0000-0003-1458-7036; Moskalenko, Igor/0000-0001-6141-458X; Mazziotta, Mario /0000-0001-9325-4672; Torres, Diego/0000-0002-1522-9065; Rando, Riccardo/0000-0001-6992-818X; Starck, Jean-Luc/0000-0003-2177-7794; Thompson, David/0000-0001-5217-9135; lubrano, pasquale/0000-0003-0221-4806; Morselli, Aldo/0000-0002-7704-9553; Foschini, Luigi/0000-0001-8678-0324; giglietto, nicola/0000-0002-9021-2888 FU National Aeronautics and Space Administration; Department of Energy in the United States; Commissariat al' Energie Atomique; Centre National de la Recherche Scientifique/Institut National de Physique Nucleaire et de Physique des Particules in France; Agenzia Spaziale Italiana; Istituto Nazionale di Fisica Nucleare in Italy; Ministry of Education, Culture, Sports, Science and Technology (MEXT); High Energy Accelerator Research Organization (KEK); Japan Aerospace Exploration Agency (JAXA) in Japan; K.A. Wallenberg Foundation; Swedish Research Council; Swedish National Space Board in Sweden; Istituto Nazionale di Astrofisica in Italy; K.A. Wallenberg Foundation in Sweden; Royal Swedish Academy of Sciences; Commonwealth of Australia FX The Fermi/LAT Collaboration acknowledges generous ongoing support from a number of agencies and institutes that have supported both the development and the operation of the LAT as well as scientific data analysis. These include the National Aeronautics and Space Administration and the Department of Energy in the United States, the Commissariat al' Energie Atomique and the Centre National de la Recherche Scientifique/Institut National de Physique Nucleaire et de Physique des Particules in France, the Agenzia Spaziale Italiana and the Istituto Nazionale di Fisica Nucleare in Italy, the Ministry of Education, Culture, Sports, Science and Technology (MEXT), High Energy Accelerator Research Organization (KEK) and Japan Aerospace Exploration Agency (JAXA) in Japan, and the K.A. Wallenberg Foundation, the Swedish Research Council and the Swedish National Space Board in Sweden.; Additional support for science analysis during the operations phase from the following agencies is also gratefully acknowledged: the Istituto Nazionale di Astrofisica in Italy and the K.A. Wallenberg Foundation in Sweden for providing a grant in support of a Royal Swedish Academy of Sciences Research fellowship for J.C.; The Australia Telescope Compact Array and Long Baseline Array are part of the Australia Telescope which is funded by the Commonwealth of Australia for operation as a National Facility managed by CSIRO. We thank the rest of the TANAMI team for their efforts that led to the observations reported here.; This research has made use of the NASA/IPAC Extragalactic Database (NED) which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. This research has made use of data obtained from the High Energy Astrophysics Science Archive Research Center (HEASARC), provided by NASA's Goddard Space Flight Center. NR 47 TC 25 Z9 25 U1 3 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD MAY 20 PY 2009 VL 697 IS 1 BP 934 EP 941 DI 10.1088/0004-637X/697/1/934 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 441JB UT WOS:000265764000080 ER PT J AU Kimura, Y Nuth, JA AF Kimura, Yuki Nuth, Joseph A., III TI A SEED OF SOLAR FORSTERITE AND POSSIBLE NEW EVOLUTIONAL SCENARIO OF COSMIC SILICATES SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE dust, extinction; infrared: solar system; infrared: stars; methods: laboratory; solar system: general; stars: AGB and post-AGB ID INTERPLANETARY DUST PARTICLES; DIFFUSE INTERSTELLAR-MEDIUM; EVOLVED STARS; CRYSTALLINE SILICATES; GRAINS; CONDENSATION; SPECTRA AB Laboratory experiments suggest that magnesium silicide (Mg(2)Si) grains could be produced in the hydrogen dominant gas outflow from evolved stars in addition to amorphous oxide minerals. If the magnesium silicide grains were incorporated into the primitive solar nebula, the magnesium silicide would easily become forsterite (Mg(2)SiO(4)) by oxidation as it reacted with the relatively oxygen-rich, solar composition gas. This hypothesis can explain the existence of abundant forsterite grains with solar oxygen composition in meteorites, i.e., magnesium silicide could be the precursor of much of the forsterite found in our solar system. In addition, if a significant fraction of the solar forsterite is derived from magnesium silicide, it could explain the apparent low abundance of presolar forsterite. Furthermore, the lower degree of crystallinity observed in silicates formed in outflows of lower mass-loss-rate stars might be caused by the formation of magnesium silicide in this relatively hydrogen-rich environment. C1 [Kimura, Yuki] Tohoku Univ, Grad Sch Sci, Dept Earth & Planetary Mat Sci, Aoba Ku, Sendai, Miyagi 9808578, Japan. [Nuth, Joseph A., III] NASA, Goddard Space Flight Ctr, Astrochem Lab, Greenbelt, MD 20771 USA. RP Kimura, Y (reprint author), Tohoku Univ, Grad Sch Sci, Dept Earth & Planetary Mat Sci, Aoba Ku, Aramaki Aoba 6-3, Sendai, Miyagi 9808578, Japan. EM ykimura@lowtem.hokudai.ac.jp RI Nuth, Joseph/E-7085-2012; Kimura, Yuki/J-9635-2014 OI Kimura, Yuki/0000-0002-9218-7663 FU Japan Society for the Promotion of Science (JSPS) [19840048]; Tohuku University FX TEM analysis was performed in the Electron Microbeam Analyses Facility of the Department of Earth and Planetary Sciences at the University of New Mexico, where Adrian J. Brearley and Ying-Bing Jiang provided technical support. This work was partially supported by grants from the Japan Society for the Promotion of Science (JSPS) Postdoctoral Fellowships for Research Abroad from 2004 April to 2006 March and a Grant-in-Aid for Young Scientists (start-up) from KAKEHI ( 19840048) of JSPS from 2006 April to 2008 March. This work was also supported in part by Tohuku University Global COE program for the "Global Education and Research Center for Earth and Planetary Dynamics". NR 25 TC 5 Z9 5 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD MAY 20 PY 2009 VL 697 IS 1 BP L10 EP L13 DI 10.1088/0004-637X/697/1/L10 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 439WX UT WOS:000265659400003 ER PT J AU Leamon, RJ McIntosh, SW AF Leamon, Robert J. McIntosh, Scott W. TI HOW THE SOLAR WIND TIES TO ITS PHOTOSPHERIC ORIGINS SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE solar wind; Sun: corona; Sun: magnetic fields; Sun: transition region ID MAGNETIC-FIELDS; CORONAL HOLE; FLUX; ACCELERATION; SPACECRAFT; SPEED AB We present a new method of visualizing the solar photospheric magnetic field based on the "Magnetic Range of Influence" (MRoI). The MRoI is a simple realization of the magnetic environment in the photosphere, reflecting the distance required to balance the integrated magnetic field contained in any magnetogram pixel. It provides a new perspective on where subterrestrial field lines in a Potential Field Source Surface (PFSS) model connect to the photosphere, and thus the source of Earth-directed solar wind ( within the limitations of PFSS models), something that is not usually obvious from a regular synoptic magnetogram. In each of three sample solar rotations, at different phases of the solar cycle, the PFSS footpoint either jumps between isolated areas of high MRoI or moves slowly within one such area. Footpoint motions are consistent with Fisk's interchange reconnection model. C1 [Leamon, Robert J.] NASA, Goddard Space Flight Ctr, Adnet Syst Inc, Greenbelt, MD 20771 USA. [McIntosh, Scott W.] Natl Ctr Atmospher Res, High Altitude Observ, Boulder, CO 80307 USA. RP Leamon, RJ (reprint author), NASA, Goddard Space Flight Ctr, Adnet Syst Inc, Code 671-1, Greenbelt, MD 20771 USA. EM robert.j.leamon@nasa.gov; mscott@ucar.edu FU National Aeronautics and Space Administration [NNH08CC02C, NNX08AU30G]; National Science Foundation FX The work presented in this Letter was supported by the National Aeronautics and Space Administration under grants issued from the Living with a Star Targeted Research & Technology Program (NNH08CC02C to R.J.L. and NNX08AU30G to S. W. M.). SOHO is a mission of international cooperation between ESA and NASA. The National Center for Atmospheric Research is sponsored by the National Science Foundation. NR 22 TC 10 Z9 10 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD MAY 20 PY 2009 VL 697 IS 1 BP L28 EP L32 DI 10.1088/0004-637X/697/1/L28 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 439WX UT WOS:000265659400007 ER PT J AU Takei, D Tsujimoto, M Kitamoto, S Ness, JU Drake, JJ Takahashi, H Mukai, K AF Takei, D. Tsujimoto, M. Kitamoto, S. Ness, J. -U. Drake, J. J. Takahashi, H. Mukai, K. TI SUZAKU DETECTION OF SUPERHARD X-RAY EMISSION FROM THE CLASSICAL NOVA V2491 CYGNI SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE novae, cataclysmic variables; stars: individual (Nova Cygni 2008 number 2, V2491 Cygni); X-rays: stars ID BOARD SUZAKU; RS-OPHIUCHI; V2362 CYGNI; SWIFT; SPECTROSCOPY; OUTBURST; MODELS; PLASMA; HXD AB We report the detection of superhard (> 10 keV) X-ray emission extending up to 70 keV from the classical nova V2491 Cygni using the Suzaku observatory. We conducted two similar to 20 ks target-of-opportunity observations 9 and 29 days after the outburst on 2008 April 11, yielding wide energy range spectra by combining the X-ray Imaging Spectrometer and the Hard X-ray Detector. On day 9, a spectrum was obtained at 1.0-70 keV with the Fe xxv K alpha line feature and a very flat continuum, which is explained by thermal plasma with a 3 keV temperature and power-law emission with a photon index of 0.1 attenuated by a heavy extinction of 1.4 x 10(23) cm(-2). The 15-70 keV luminosity at 10.5 kpc is 6 x 10(35) erg s(-1). The superhard emission was not present on day 29. This is the highest energy at which X-rays have been detected from a classical nova. We argue a nonthermal origin for the emission, which suggests the presence of accelerated charged particles in the nova explosion. C1 [Takei, D.; Kitamoto, S.] Rikkyo Univ, Dept Phys, Toshima Ku, Tokyo 1718501, Japan. [Tsujimoto, M.] Japan Aerosp Explorat Agcy, Inst Space & Astronaut Sci, Sagamihara, Kanagawa 2298510, Japan. [Tsujimoto, M.] Penn State Univ, Dept Astron & Astrophys, Davey Lab 525, University Pk, PA 16802 USA. [Ness, J. -U.] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85287 USA. [Ness, J. -U.] European Space Agcy, XMM Newton Observ SOC, SRE OAX, Madrid 28691, Spain. [Drake, J. J.] SAO, Cambridge, MA 02138 USA. [Takahashi, H.] Hiroshima Univ, Sch Sci, Dept Phys Sci, Hiroshima 7398526, Japan. [Mukai, K.] NASA, Goddard Space Flight Ctr, CRESST & Xray Astrophys Lab, Greenbelt, MD 20771 USA. [Mukai, K.] Univ Maryland Baltimore Cty, Dept Phys, Baltimore, MD 21250 USA. RP Takei, D (reprint author), Rikkyo Univ, Dept Phys, Toshima Ku, 3-34-1 Nishi Ikebukuro, Tokyo 1718501, Japan. EM akei@ast.rikkyo.ac.jp RI XRAY, SUZAKU/A-1808-2009 FU NASA [PF6-70044, PF5-60039, NAS8-03060, NAS8-39073] FX The authors appreciate the reviewer, Klaus Beuermann, for useful suggestions. We also thank the Suzaku telescope managers for the director's discretionary time and I. Hachisu, M. Kato, K. Kinugasa, H. Murakami, and M. Morii for comments. D. T. is financially supported by the Japan Society for the Promotion of Science. Support for this work was provided by the NASA through Chandra Postdoctoral Fellowship Awards (PF6-70044, M. T.; PF5-60039, J.-U.N.) operated by the SAO for and on behalf of the NASA under contract NAS8-03060. J.J.D. was supported by the NASA contract NAS8-39073. NR 44 TC 10 Z9 10 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD MAY 20 PY 2009 VL 697 IS 1 BP L54 EP L57 DI 10.1088/0004-637X/697/1/L54 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 439WX UT WOS:000265659400012 ER PT J AU Farrell, WM Kurth, WS Gurnett, DA Johnson, RE Kaiser, ML Wahlund, JE Waite, JH AF Farrell, W. M. Kurth, W. S. Gurnett, D. A. Johnson, R. E. Kaiser, M. L. Wahlund, J. -E. Waite, J. H., Jr. TI Electron density dropout near Enceladus in the context of water-vapor and water-ice SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID NEUTRAL MASS-SPECTROMETER; PLASMA-WAVE INSTRUMENT; CASSINI RADIO; SATURN; ION; MAGNETOSPHERE; PLUME; RING; OH AB On 12 March 2008, the Cassini spacecraft made a close encounter with the Saturnian moon Enceladus, passing within 52 km of the moon. The spacecraft trajectory was intentionally-oriented in a southerly direction to create a close alignment with the intense water-dominated plumes emitted from the south polar region. During the passage, the Cassini Radio and Plasma Wave System (RPWS) detected two distinct radio signatures: 1) Impulses associated with small water-ice dust grain impacts and 2) an upper hybrid (UH) resonance emission that both intensified and displayed a sharp frequency decrease in the near-vicinity of the moon. The frequency decrease of the UH emission is associated with an unexpectedly sharp decrease in electron density from similar to 90 cl/cm(3) to below 20 cl/cm(3) that occurs on a time scale of a minute near the closest encounter with the moon. In this work, we consider a number of scenarios to explain this sharp electron dropout, but surmise that electron absorption by ice grains is the most likely process. Citation: Farrell, W. M., W. S. Kurth, D. A. Gurnett, R. E. Johnson, M. L. Kaiser, J.-E. Wahlund, and J. H. Waite Jr. (2009), Electron density dropout near Enceladus in the context of water-vapor and water-ice, Geophys. Res. Lett., 36, L10203, doi: 10.1029/2008GL037108. C1 [Farrell, W. M.; Kaiser, M. L.] NASA, Goddard Space Flight Ctr, Space Explorat Directorate, Greenbelt, MD 20771 USA. [Kurth, W. S.; Gurnett, D. A.] Univ Iowa, Dept Phys & Astron, Iowa City, IA 52242 USA. [Johnson, R. E.] Univ Virginia, Dept Mat Sci & Engn, Charlottesville, VA 22903 USA. [Wahlund, J. -E.] Swedish Inst Space Phys, SE-75121 Uppsala, Sweden. [Waite, J. H., Jr.] SW Res Inst, San Antonio, TX 78238 USA. RP Farrell, WM (reprint author), NASA, Goddard Space Flight Ctr, Space Explorat Directorate, Code 695, Greenbelt, MD 20771 USA. EM william.farrell@gsfc.nasa.gov RI Farrell, William/I-4865-2013; OI Kurth, William/0000-0002-5471-6202 NR 29 TC 33 Z9 33 U1 1 U2 3 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD MAY 20 PY 2009 VL 36 AR L10203 DI 10.1029/2008GL037108 PG 5 WC Geosciences, Multidisciplinary SC Geology GA 449XB UT WOS:000266362900001 ER PT J AU Watson, A Ramirez, CV Salud, E AF Watson, Andrew Ramirez, Cesar V. Salud, Ellen TI Predicting Visibility of Aircraft SO PLOS ONE LA English DT Article ID CONTRAST-SENSITIVITY; VISION RESEARCH; PERFORMANCE; QUEST AB Visual detection of aircraft by human observers is an important element of aviation safety. To assess and ensure safety, it would be useful to be able to be able to predict the visibility, to a human observer, of an aircraft of specified size, shape, distance, and coloration. Examples include assuring safe separation among aircraft and between aircraft and unmanned vehicles, design of airport control towers, and efforts to enhance or suppress the visibility of military and rescue vehicles. We have recently developed a simple metric of pattern visibility, the Spatial Standard Observer (SSO). In this report we examine whether the SSO can predict visibility of simulated aircraft images. We constructed a set of aircraft images from three-dimensional computer graphic models, and measured the luminance contrast threshold for each image from three human observers. The data were well predicted by the SSO. Finally, we show how to use the SSO to predict visibility range for aircraft of arbitrary size, shape, distance, and coloration. RP Watson, A (reprint author), NASA, Ames Res Ctr, Moffett Field, VA USA. EM Andrew.b.watson@nasa.gov NR 25 TC 4 Z9 4 U1 2 U2 5 PU PUBLIC LIBRARY SCIENCE PI SAN FRANCISCO PA 1160 BATTERY STREET, STE 100, SAN FRANCISCO, CA 94111 USA SN 1932-6203 J9 PLOS ONE JI PLoS One PD MAY 20 PY 2009 VL 4 IS 5 AR e5594 DI 10.1371/journal.pone.0005594 PG 16 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 448AY UT WOS:000266234700007 PM 19462007 ER PT J AU Yang, K Liu, X Krotkov, NA Krueger, AJ Carn, SA AF Yang, Kai Liu, Xiong Krotkov, Nickolay A. Krueger, Arlin J. Carn, Simon A. TI Estimating the altitude of volcanic sulfur dioxide plumes from space borne hyper-spectral UV measurements SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID OZONE PROFILES; ERUPTION; SPECTROMETER; TRACKING; DOAS; SO2 AB The altitude of volcanic sulfur dioxide (SO2) plumes determines the transport and atmospheric residence time of derived sulfate aerosol, and hence their impacts on the environment and climate. Knowledge of the altitude of fresh eruption clouds is also very important in aviation safety to avoid flying through ash clouds and for forecasting of plume drift. In this paper, we demonstrate the altitude dependence of the spectral response in the backscattered ultraviolet (BUV) radiance when a SO2 absorption layer is added to an ozone-laden atmosphere. The distinctive spectral response serves as the physical basis for simultaneous SO2 loading and altitude retrievals, which can improve the characterization of volcanic emissions. We accomplish this by extending the recently developed Iterative Spectral Fitting (ISF) algorithm to include effective plume altitude determination when performing simultaneous ozone and SO2 retrievals. The extended ISF algorithm is applied to hyper-spectral Ozone Monitoring Instrument (OMI) measurements of two volcanic eruptions: Sierra Negra in October 2005 and Jebel al Tair in September 2007. The results show for the first time that a wide range of SO2 plume altitudes can be estimated directly from hyperspectral BUV radiance measurements. Citation: Yang, K., X. Liu, N. A. Krotkov, A. J. Krueger, and S. A. Carn (2009), Estimating the altitude of volcanic sulfur dioxide plumes from space borne hyper-spectral UV measurements, Geophys. Res. Lett., 36, L10803, doi: 10.1029/2009GL038025. C1 [Yang, Kai; Liu, Xiong; Krotkov, Nickolay A.] Univ Maryland Baltimore Cty, GEST, Baltimore, MD 21228 USA. [Carn, Simon A.] Michigan Technol Univ, Dept Geol & Min Engn & Sci, Houghton, MI 49931 USA. [Krueger, Arlin J.] Univ Maryland Baltimore Cty, JCET, Baltimore, MD 21250 USA. [Yang, Kai; Liu, Xiong; Krotkov, Nickolay A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Yang, K (reprint author), Univ Maryland Baltimore Cty, GEST, Baltimore, MD 21228 USA. EM kai.yang-1@nasa.gov RI Krotkov, Nickolay/E-1541-2012; Liu, Xiong/P-7186-2014 OI Krotkov, Nickolay/0000-0001-6170-6750; Liu, Xiong/0000-0003-2939-574X FU NASA [NNS06AA05G] FX This work was supported in part by NASA under grant NNS06AA05G (NASA volcanic cloud data for aviation hazards). NR 16 TC 28 Z9 28 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 MAY 19 PY 2009 VL 36 AR L10803 DI 10.1029/2009GL038025 PG 6 WC Geosciences, Multidisciplinary SC Geology GA 449WX UT WOS:000266362500006 ER PT J AU Arumugam, PU Chen, H Siddiqui, S Weinrich, JAP Jejelowo, A Li, J Meyyappan, M AF Arumugam, Prabhu U. Chen, Hua Siddiqui, Shabnam Weinrich, Jarret A. P. Jejelowo, Ayodeji Li, Jun Meyyappan, M. TI Wafer-scale fabrication of patterned carbon nanofiber nanoelectrode arrays: A route for development of multiplexed, ultrasensitive disposable biosensors SO BIOSENSORS & BIOELECTRONICS LA English DT Article DE Vertically aligned carbon nanofibers; Multiplexed electrochemical detection; Nanoelectrode array; Ultrasensitive nucleic acid detection; Biosensor ID LABEL-FREE; DNA; ELECTRODES AB One of the major limitations in the development of ultrasensitive electrochemical biosensors based on one-dimensional nanostructures is the difficulty involved with reliably fabricating nanoelectrode arrays (NEAs). In this work, we describe a simple, robust and scalable wafer-scale fabrication method to produce multiplexed biosensors. Each sensor chip consists of nine individually addressable arrays that uses electron beam patterned vertically aligned carbon nanofibers (VACNFs) as the sensing element. To ensure nanoelectrode behavior with higher sensitivity, VACNFs were precisely grown on 100 nm Ni dots with 1 mu m spacing on each micro pad. Pretreatments by the combination of soaking in 1.0 M HNO(3) and electrochemical etching in 1.0 M NaOH dramatically improved the electrode performance, indicated by the decrease of redox peak separation in cyclic voltammograrn (Delta E(p)) to similar to 100 mV and an approximately 200% increase in steady-state currents. The electrochemical detection of the hybridization of DNA targets from E coli O157:H7 onto oligonucleotide probes were successfully demonstrated. The 9 arrays within the chip were divided into three groups with triplicate sensors for positive control, negative control and specific hybridization. The proposed method has the potential to be scaled up to N x N arrays with N up to 10, which is ideal for detecting a myriad of organisms. In addition, such sensors can be used as a generic platform for many electroanalysis applications. (C) 2009 Elsevier B.V. All rights reserved. C1 [Arumugam, Prabhu U.; Chen, Hua; Siddiqui, Shabnam; Meyyappan, M.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Li, Jun] Kansas State Univ, Dept Chem, Manhattan, KS 66506 USA. [Weinrich, Jarret A. P.] Univ Miami, Coral Gables, FL 33124 USA. [Jejelowo, Ayodeji] Johns Hopkins Univ, Baltimore, MD USA. RP Arumugam, PU (reprint author), NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. EM prabhu.u.arumugam@nasa.gov; hua.chen-1@nasa.gov RI Li, Jun/H-7771-2013 OI Li, Jun/0000-0002-3689-8946 FU Early Warning Inc., Troy, NY [NAS2-03144]; NASA Ames Research Center; University Affiliated Research Center (UARC); University of California; Santa Cruz and Eloret Corporation; NASA Undergraduate Student Research Program and JAPFA, Inc., Humble, TX FX This work was funded by Early Warning Inc., Troy, NY, under the supervision of Neil Gordon via contract number NAS2-03144 (Task TO.066.0.HP.TSN) to NASA Ames Research Center, University Affiliated Research Center (UARC), University of California, Santa Cruz and Eloret Corporation. Early Warning has related patents pending. PUA and HC are employed by ELORET Corporation; SS is employed by Education Associates, onsite contractors at NASA Ames. JAPW and AJ are undergraduate students from University of Miami, and Johns Hopkins University, respectively and their work is supported by NASA Undergraduate Student Research Program and JAPFA, Inc., Humble, TX. We thank Professor Bruce Gale and his students at the University of Utah for optical lithography patterning of micro pads and Dr. Xuhui Sun of Center for Nanostructures, Santa Clara University, CA for helpful discussions on CNF growth. NR 26 TC 59 Z9 59 U1 1 U2 21 PU ELSEVIER ADVANCED TECHNOLOGY PI OXFORD PA OXFORD FULFILLMENT CENTRE THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 0956-5663 J9 BIOSENS BIOELECTRON JI Biosens. Bioelectron. PD MAY 15 PY 2009 VL 24 IS 9 BP 2818 EP 2824 DI 10.1016/j.bios.2009.02.009 PG 7 WC Biophysics; Biotechnology & Applied Microbiology; Chemistry, Analytical; Electrochemistry; Nanoscience & Nanotechnology SC Biophysics; Biotechnology & Applied Microbiology; Chemistry; Electrochemistry; Science & Technology - Other Topics GA 447LP UT WOS:000266192900010 PM 19303281 ER PT J AU Furst, F Wilms, J Rothschild, RE Pottschmidt, K Smith, DM Lingenfelter, R AF Fuerst, Felix Wilms, Joern Rothschild, Richard E. Pottschmidt, Katja Smith, David M. Lingenfelter, Richard TI Temporal variations of strength and location of the South Atlantic Anomaly as measured by RXTE SO EARTH AND PLANETARY SCIENCE LETTERS LA English DT Article DE space radiation environment; South Atlantic Anomaly; radiation monitors; Rossi X-ray Timing Explorer ID GEOMAGNETIC SECULAR VARIATION; RADIATION ENVIRONMENT; SATELLITE DATA; SPACE; JERK; FLOWS; STORM; CORE; MIR AB The evolution of the particle background at an altitude of similar to 540 km during the time interval between 1996 and 2007 is studied using the particle monitor of the High Energy X-ray Timing Experiment on board NASA's Rossi X-ray Timing Explorer. A special emphasis of this study is the location and strength of the South Atlantic Anomaly (SAA). The size and strength of the SAA are anti-correlated with the 10.7 cm radio flux of the Sun, which leads the SAA strength by similar to 1 year reflecting variations in solar heating of the upper atmosphere. The location of the SAA is also found to drift westwards with an average drift rate of about 0.3 degrees/yr following the drift of the geomagnetic-field configuration. Superimposed to this drift rate are irregularities, where the SAA suddenly moves eastwards and where furthermore the speed of the drift changes. The most prominent of these irregularities is found in the second quarter of 2003 and another event took place in 1999. We suggest that these events are previously unrecognized manifestations of the geomagnetic jerks of the Earth's magnetic field. (c) 2009 Elsevier B.V. All rights reserved. C1 [Fuerst, Felix; Wilms, Joern] Erlangen Ctr Astroparticle Phys, D-91058 Erlangen, Germany. [Fuerst, Felix; Wilms, Joern] Dr Karl Remeis Sternwarte, D-96049 Bamberg, Germany. [Rothschild, Richard E.; Pottschmidt, Katja; Lingenfelter, Richard] Univ Calif San Diego, Ctr Astrophys & Space Sci, La Jolla, CA 92093 USA. [Pottschmidt, Katja] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA. [Pottschmidt, Katja] CRESST, Greenbelt, MD 20771 USA. [Pottschmidt, Katja] Univ Maryland Baltimore Cty, Ctr Space Sci & Technol, Baltimore, MD 21250 USA. [Smith, David M.] Univ Calif Santa Cruz, SCIPP, Santa Cruz, CA 95064 USA. RP Furst, F (reprint author), Erlangen Ctr Astroparticle Phys, Erwin Rommel Str 1, D-91058 Erlangen, Germany. EM felix.fuerst@sternwarte.uni-erlangen.de; joern.wilms@sternwarte.uni-erlangen.de; rrothschild@ucsd.edu; katja@milkyway.gsfc.nasa.gov; dsmith@scipp.ucsc.edu; rlingenfelter@ucsd.edu RI Wilms, Joern/C-8116-2013 OI Wilms, Joern/0000-0003-2065-5410 FU Deutsches Zentrum fur Luft- und Raumfahrt [50OR8080, 50QR0801]; National Aeronautics and Space Administration [NAG5-30720]; Deutscher Akademischer Austauschdienst [D/06/29438] FX We acknowledge partial support from Deutsches Zentrum fur Luft- und Raumfahrt grants 50OR8080 and 50QR0801, from National Aeronautics and Space Administration grant NAG5-30720, and from Deutscher Akademischer Austauschdienst travel grant D/06/29438. We thank the complete RXTE team, especially the HEXTE team, for their support. We also thank the referees for their very helpful comments. NR 37 TC 19 Z9 19 U1 0 U2 3 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 MAY 15 PY 2009 VL 281 IS 3-4 BP 125 EP 133 DI 10.1016/j.epsl.2009.02.004 PG 9 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 456SQ UT WOS:000266869000001 ER PT J AU Rajaram, M Anand, SP Hemant, K Purucker, ME AF Rajaram, Mita Anand, S. P. Hemant, K. Purucker, M. E. TI Curie isotherm map of Indian subcontinent from satellite and aeromagnetic data SO EARTH AND PLANETARY SCIENCE LETTERS LA English DT Article DE Aeromagnetic data; CHAMP; Curie isotherm; spectral methods ID DEEP SEISMIC-SOUNDINGS; CRUSTAL STRUCTURE; MAGNETIC-ANOMALIES; CONTINENTAL-CRUST; BASIN; CALIFORNIA; REGIONS; PROFILE; SURFACE; MODELS AB Estimating depth to the bottom of the magnetic crust (synonymously called the Curie isotherm) on a regional scale from long wavelength magnetic anomalies requires that large areas of survey data be used for the calculations. There is still no consensus on the minimum survey area required to arrive at a reliable estimate of the Curie isotherm depth. From the available aeromagnetic data over India, depth to the Curie isotherm is estimated using spectral techniques. We found that the significant spectral maxima required to calculate the depth to the Curie isotherm existed only for 4 degrees x4 degrees blocks in southern peninsular India up to 18 degrees N latitude and for 5 degrees x5 degrees blocks for the rest of the region in Central India. As aeromagnetic data coverage over India is incomplete, we also calculate the magnetic crustal thickness from the lithospheric model of the CHAMP satellite data for the whole country, using an iterative forward modeling approach. The calculated Curie isotherm is shallow in the mobile belts and deeper in the cratons in both the derivations. As the Curie isotherms calculated from the two data sets collected at very different altitudes using totally different techniques, match reasonably well, it lends credence to the methodology adopted. The derived Curie isotherm depth map is in accordance with the basic structural trend of the major tectonic units within the Indian subcontinent. A comparison is made of the calculated Curie isotherm depth with Moho depths along available DSS profiles over India and it is found that the Curie depth is generally shallower than the Moho depth implying that it possibly represents a thermal boundary rather than a compositional change. Further, we find that high magnitude earthquakes are associated with high gradients in Curie depth. (c) 2009 Elsevier B.V. All rights reserved. C1 [Rajaram, Mita; Anand, S. P.] Indian Inst Geomagnetism, Navi Mumbai, India. [Rajaram, Mita; Hemant, K.] NASA, Goddard Space Flight Ctr, ORAU, Planetary Geodynam Lab, Greenbelt, MD USA. [Purucker, M. E.] NASA, Goddard Space Flight Ctr, Raytheon ITSS, Greenbelt, MD USA. RP Rajaram, M (reprint author), Indian Inst Geomagnetism, Navi Mumbai, India. EM mita@iigs.iigm.res.in; anand@iigs.iigm.res.in; fnu.kumarhemant-1@nasa.gov; purucker@geomag.gsfc.nasa.gov RI S P, Anand/G-8451-2011 FU NASA FX M. Rajaram wishes to thank Dr. H. Frey for providing all facilities during her visit to GSFC, NASA. K. Hemant wishes to thank NASA Postdoctoral Program (NPP) and ORAU for providing the post-doctoral fellowship to work at GSFC, NASA. We wish to thank the reviewers for their valuable comments that helped to improve the manuscript. NR 46 TC 26 Z9 29 U1 0 U2 5 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 MAY 15 PY 2009 VL 281 IS 3-4 BP 147 EP 158 DI 10.1016/j.epsl.2009.02.013 PG 12 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 456SQ UT WOS:000266869000003 ER PT J AU Schmidt, ME Farrand, WH Johnson, JR Schroder, C Hurowitz, JA Mccoy, TJ Ruff, SW Arvidson, RE Marais, DJD Lewis, KW Ming, DW Squyres, SW de Souza, PA AF Schmidt, M. E. Farrand, W. H. Johnson, J. R. Schroeder, C. Hurowitz, J. A. Mccoy, T. J. Ruff, S. W. Arvidson, R. E. Marais, D. J. Des Lewis, K. W. Ming, D. W. Squyres, S. W. de Souza, P. A., Jr. TI Spectral, mineralogical, and geochemical variations across Home Plate, Gusev Crater, Mars indicate high and low temperature alteration SO EARTH AND PLANETARY SCIENCE LETTERS LA English DT Article DE Mars geology; Gusev Crater; hydrothermal alteration ID SOILS; ROCKS; WATER; DUST AB Over the last similar to 3 years in Gusev Crater, Mars, the Spirit rover observed coherent variations in color, mineralogy, and geochemistry across Home Plate, an similar to 80 m-diameter outcrop of basaltic tephra. Observations of Home Plate from orbit and from the summit of Husband Hill reveal clear differences in visible/near-infrared (VNIR) colors between its eastern and western regions that are consistent with mineralogical compositions indicated by Mossbauer spectrometer (MB) and by Miniature Thermal Emission Spectrometer (Mini-TES). Pyroxene and magnetite dominate the east side, while olivine, nanophase Fe oxide (npOx) and glass are more abundant on the western side. Alpha Particle X-Ray Spectrometer (APXS) observations reveal that eastern Home Plate has higher Si/Mg, Al, Zn, Ni, and K, while Cl and Br are higher in the west. We propose that these variations are the result of two distinct alteration regimes that may or may not be temporally related: a localized, higher temperature recrystallization and alteration of the east side of Home Plate and lower temperature alteration of the western side that produced npOx. Published by Elsevier B.V. C1 [Schmidt, M. E.; Mccoy, T. J.] Smithsonian Inst, Dept Mineral Sci, Washington, DC 20560 USA. [Farrand, W. H.] Space Sci Inst, Boulder, CO 80301 USA. [Johnson, J. R.] US Geol Survey, Astrogeol Team, Flagstaff, AZ 86001 USA. [Schroeder, C.] Johannes Gutenberg Univ Mainz, Inst Anorgan Chem & Analyt Chem, D-55128 Mainz, Germany. [Hurowitz, J. A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Ruff, S. W.] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85287 USA. [Arvidson, R. E.] Washington Univ, Dept Earth & Planetary Sci, St Louis, MO 63130 USA. [Marais, D. J. Des] NASA, Ames Res Ctr, Exobiol Branch, Moffett Field, CA 94035 USA. [Lewis, K. W.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. [Ming, D. W.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. [Squyres, S. W.] Cornell Univ, Dept Astron, Ithaca, NY 14853 USA. [de Souza, P. A., Jr.] CSIRO, Tasmanian ICT Ctr, Hobart, Tas 7000, Australia. RP Schmidt, ME (reprint author), Smithsonian Inst, Dept Mineral Sci, Washington, DC 20560 USA. EM schmidtm@si.edu RI de Souza, Paulo/B-8961-2008; Schroder, Christian/B-3870-2009; Centre, TasICT/D-1212-2011; Lewis, Kevin/E-5557-2012; Johnson, Jeffrey/F-3972-2015 OI de Souza, Paulo/0000-0002-0091-8925; Schroder, Christian/0000-0002-7935-6039; NR 41 TC 30 Z9 30 U1 1 U2 17 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0012-821X EI 1385-013X J9 EARTH PLANET SC LETT JI Earth Planet. Sci. Lett. PD MAY 15 PY 2009 VL 281 IS 3-4 BP 258 EP 266 DI 10.1016/j.epsl.2009.02.030 PG 9 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 456SQ UT WOS:000266869000012 ER PT J AU Smith, DE Zuber, MT Torrence, MH Dunn, PJ Neumann, GA Lemoine, FG Fricke, SK AF Smith, David E. Zuber, Maria T. Torrence, Mark H. Dunn, Peter J. Neumann, Gregory A. Lemoine, Frank G. Fricke, Susan K. TI Time variations of Mars' gravitational field and seasonal changes in the masses of the polar ice caps SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Article ID GENERAL-CIRCULATION MODEL; EMISSION SPECTROMETER EXPERIMENT; ORBITER LASER ALTIMETER; GLOBAL SURVEYOR; GRAVITY-FIELD; VIKING OBSERVATIONS; MARTIAN ATMOSPHERE; CARBON-DIOXIDE; CO2 CYCLE; PRESSURE AB Tracking of the Mars Global Surveyor spacecraft has been used to measure changes in the long-wavelength gravity field of Mars and to estimate the seasonal mass of carbon dioxide that is deposited in the polar regions each fall and winter and sublimed back into the atmosphere every spring and summer. Observations spanning 4 Mars years have been analyzed. A clear and well-defined seasonal signal, composed of annual and semiannual periods, is seen in the lowest odd degree 3 coefficient but with less confidence in the lowest even degree 2, which is expected to be smaller and is also much more difficult to observe. Direct estimation of the seasonal mass exchange employing a simple, seasonally varying model of the size and height of each cap provides values that indicate some systematic departures from the deposition predicted by a general circulation model. Estimates are also obtained for the precession and nutation of the pole of rotation of Mars, the degree 2 tidal Love number, k(2), and the mass of Phobos, the larger of Mars' two natural satellites. C1 [Smith, David E.; Neumann, Gregory A.; Lemoine, Frank G.] NASA, Goddard Space Flight Ctr, Solar Syst Explorat Div, Greenbelt, MD 20771 USA. [Zuber, Maria T.] MIT, Dept Earth Atmospher & Planetary Sci, Cambridge, MA 02139 USA. [Torrence, Mark H.; Fricke, Susan K.] SGT Inc, Greenbelt, MD 20770 USA. [Dunn, Peter J.] Raytheon Informat Solut, Riverdale, MD 20737 USA. RP Smith, DE (reprint author), NASA, Goddard Space Flight Ctr, Solar Syst Explorat Div, Code 690, Greenbelt, MD 20771 USA. EM dsmith@tharsis.gsfc.nasa.gov; zuber@mit.edu; Mark.H.Torrence.1@nasa.gov; gregory.a.neumann@nasa.gov; frank.g.lemoine@nasa.gov; Susan.K.Fricke@nasa.gov RI Lemoine, Frank/D-1215-2013; Neumann, Gregory/I-5591-2013 OI Neumann, Gregory/0000-0003-0644-9944 FU Mars Global Survey FX This work was supported by the Mars Global Survey or Project of the NASA Mars Program. We thank David Rowlands for software development and Robert Haberle for providing the Ames GCM simulation used in the analysis. NR 59 TC 16 Z9 17 U1 1 U2 3 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 MAY 15 PY 2009 VL 114 AR E05002 DI 10.1029/2008JE003267 PG 15 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 446DW UT WOS:000266101600001 ER PT J AU Kang, JH Park, C Scholl, JA Brazin, AH Holloway, NM High, JW Lowther, SE Harrison, JS AF Kang, Jin Ho Park, Cheol Scholl, Jonathan A. Brazin, Amy H. Holloway, Nancy M. High, James W. Lowther, Sharon E. Harrison, Joycelyn S. TI Piezoresistive Characteristics of Single Wall Carbon Nanotube/Polyimide Nanocomposites SO JOURNAL OF POLYMER SCIENCE PART B-POLYMER PHYSICS LA English DT Article DE carbon nanotubes; composites; high performance polymers; piezoresistance; polyimides ID NANOTUBE-POLYMER COMPOSITES; PIEZOELECTRIC PROPERTIES; POLYIMIDE; SENSOR; FIBER; CONDUCTIVITY; ELECTRODES; DISPERSION; ALUMINUM; STRAIN AB A systematic study of the effect of single wall carbon nanotubes (SWCNTs) on the enhanced piezoresistive sensitivity of polyimide nanocomposites from below to above percolation was accomplished. The maximum piezoresistive stress coefficient (Pi) of 1.52 x 10(-3) MPa(-1) was noted at just above the percolation threshold concentration (Phi similar to 0.05 wt %) of SWCNT. This coefficient value exceeds those of metallic piezoresistive materials by two orders of magnitude (4.25 x 10(-5) MPa(-1) for aluminum). The high piezoresistive characteristics appear to originate from a change in the intrinsic resistivity of the composite caused by the variation of the tunneling distance between conducting inclusions (SWCNTs) under compression or tension. (C) 2009 Wiley Periodicals, Inc.* J Polym Sci Part B: Polym Phys 47: 994-1003, 2009 C1 [Kang, Jin Ho; Park, Cheol] Natl Inst Aerosp, Hampton, VA 23681 USA. [Park, Cheol] Univ Virginia, Dept Mech & Aerosp Engn, Charlottesville, VA 22904 USA. [Scholl, Jonathan A.] Princeton Univ, Dept Chem Engn, Princeton, NJ 08544 USA. [Brazin, Amy H.] MIT, Cambridge, MA 02139 USA. [Holloway, Nancy M.] NASA, Langley Res Ctr, Fabricat Technol Dev Branch, Elect Applicat Technol Sect, Hampton, VA 23681 USA. [High, James W.] NASA, Langley Res Ctr, Elect Syst Branch, Hampton, VA 23681 USA. [Lowther, Sharon E.; Harrison, Joycelyn S.] NASA, Langley Res Ctr, Adv Mat & Proc Branch, Hampton, VA 23681 USA. RP Kang, JH (reprint author), Natl Inst Aerosp, MS 226,6 W Taylor St, Hampton, VA 23681 USA. EM jin.h.kang@nasa.gov; Cheol.Park-1@nasa.gov NR 37 TC 52 Z9 53 U1 2 U2 25 PU JOHN WILEY & SONS INC PI HOBOKEN PA 111 RIVER ST, HOBOKEN, NJ 07030 USA SN 0887-6266 J9 J POLYM SCI POL PHYS JI J. Polym. Sci. Pt. B-Polym. Phys. PD MAY 15 PY 2009 VL 47 IS 10 BP 994 EP 1003 DI 10.1002/polb.21705 PG 10 WC Polymer Science SC Polymer Science GA 440KS UT WOS:000265699800005 ER PT J AU Sobieski, P Craeye, C Bliven, LF AF Sobieski, P. Craeye, C. Bliven, L. F. TI A relationship between rain radar reflectivity and height elevation variance of ringwaves due to the impact of rain on the sea surface SO RADIO SCIENCE LA English DT Article ID TRMM PRECIPITATION RADAR; DROP-SIZE DISTRIBUTION; KU-BAND BACKSCATTER; WATER SURFACES; RING-WAVES; ARTIFICIAL RAIN; SCATTEROMETER; SCATTERING; WIND; DISTRIBUTIONS AB Raindrops impacting the rough sea modify its surface and its backscattering coefficient. This roughness change essentially depends on the rain content in very large drops, which is highly variable from one drop size distribution model to another. However, it has been observed that the radar reflectivity of raindrops has a drop size dependence very similar to that of the ringwaves induced by rain on the surface. From a numerical analysis on various drop size distributions, rain rates, and frequencies from 3 to 35 GHz, a relationship between the sea surface elevation variance of ringwaves resulting from drop impact and the rain radar reflectivity Z is established. It is found to be weakly dependent on the raindrop size distribution model. This link is expected to lead to better estimates of the surface roughness, and in turn, via electromagnetic scattering models, it could improve algorithms for near nadir rain radar retrieval. C1 [Sobieski, P.; Craeye, C.] Catholic Univ Louvain, Telecommun & Remote Sensing Lab, B-1348 Louvain, Belgium. [Bliven, L. F.] NASA, Goddard Space Flight Ctr, Wallops Flight Facil, Wallops Isl, VA 23337 USA. RP Sobieski, P (reprint author), Catholic Univ Louvain, Telecommun & Remote Sensing Lab, B-1348 Louvain, Belgium. EM piotr.sobieski@uclouvain.be; christophe.craeye@uclouvain.be; francis.l.bliven@nasa.gov RI bliven, francis/E-1450-2012 NR 70 TC 4 Z9 4 U1 0 U2 2 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0048-6604 EI 1944-799X J9 RADIO SCI JI Radio Sci. PD MAY 15 PY 2009 VL 44 AR RS3005 DI 10.1029/2008RS003880 PG 20 WC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology & Atmospheric Sciences; Remote Sensing; Telecommunications SC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology & Atmospheric Sciences; Remote Sensing; Telecommunications GA 446ES UT WOS:000266104000001 ER PT J AU Chander, G Markham, BL Helder, DL AF Chander, Gyanesh Markham, Brian L. Helder, Dennis L. TI Summary of current radiometric calibration coefficients for Landsat MSS, TM, ETM+, and EO-1 ALI sensors SO REMOTE SENSING OF ENVIRONMENT LA English DT Article DE Landsat MSS, TM, ETM; EO-1 ALI; Radiometric characterization & calibration; At-sensor spectral radiance; Top-of-atmosphere reflectance; At-sensor brightness temperature ID REFLECTANCE-BASED METHOD; THEMATIC MAPPER DATA; CROSS-CALIBRATION; SPECTRAL CHARACTERIZATION; UNITED-STATES; RECORD AB This paper provides a summary of the current equations and rescaling factors for converting calibrated Digital Numbers (DNs) to absolute units of at-sensor spectral radiance. Top-Of-Atmosphere (TOA) reflectance, and at-sensor brightness temperature. It tabulates the necessary constants for the Multispectral Scanner (MSS), Thematic Mapper (TM), Enhanced Thematic Mapper Plus (ETM+), and Advanced Land Imager (ALI) sensors. These conversions provide a basis for standardized comparison of data in a single scene or between images acquired on different dates or by different sensors. This paper forms a needed guide for Landsat data users who now have access to the entire Landsat archive at no cost. (C) 2009 Elsevier Inc. All rights reserved. C1 [Chander, Gyanesh] SGT Inc, Sioux Falls, SD 57198 USA. [Markham, Brian L.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Helder, Dennis L.] S Dakota State Univ, Brookings, SD 57007 USA. RP Chander, G (reprint author), SGT Inc, Sioux Falls, SD 57198 USA. EM gchander@usgs.gov RI Markham, Brian/M-4842-2013 OI Markham, Brian/0000-0002-9612-8169 FU NASA Land-Cover and Land-Use Change (LCLUC) [NNH08AI301] FX This work was partially supported by the NASA Land-Cover and Land-Use Change (LCLUC) Grant NNH08AI301. The authors acknowledge the support of David Aaron (SDSU) for digitizing the spectral responses for the MSS sensors and Julia Barsi (SSAI) for generating the Earth-Sun distance. Special thanks are extended to a number of colleagues for reviewing drafts of this manuscript. The anonymous reviewers' comments were particularly valuable and their efforts are greatly appreciated. Any use of trade, product, or firm names is for descriptive purposes only and does not imply endorsement by the U.S. Government. NR 56 TC 829 Z9 939 U1 30 U2 170 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 MAY 15 PY 2009 VL 113 IS 5 BP 893 EP 903 DI 10.1016/j.rse.2009.01.007 PG 11 WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic Technology SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science & Photographic Technology GA 440QY UT WOS:000265716000002 ER PT J AU Tedesco, M AF Tedesco, M. TI Assessment and development of snowmelt retrieval algorithms over Antarctica from K-band spaceborne brightness temperature (1979-2008) SO REMOTE SENSING OF ENVIRONMENT LA English DT Article DE Antarctica; Snowmelt; Passive microwave ID ONSET; SURFACE; DURATION AB Results from several previously published algorithms for wet snow detection in Antarctica from K-band spaceborne brightness temperature are compared and evaluated vs. estimates of wet snow conditions from ground measurements. In addition, a new physically-driven algorithm, in which the detectable liquid water content is assumed constant, is proposed and assessed. All algorithms are also evaluated by analyzing their results during collapses of ice shelves. Two algorithms are selected for deriving updated trends of melting index (MI, the number of melting days times the area subject to melting) between 1979 and 2008 over the whole Antarctica and at sub-continental scales. In the first algorithm wet snow is identified when brightness temperature exceeds the mean of winter brightness temperature plus 30 K and the second is the new model-based approach described here. Both negative and positive MI trends are obtained, depending on the algorithm used. A high number of melting days (up to 100 days) are detected over the Wilkins ice shelf, the Peninsula and the George VI ice shelf. Over East Antarctica, the West and Amery ice shelves are subject to melting for a maximum of approximately 50 days. Positive trends of number of melting days are detected over most of the West Antarctica, with peak values up to 1.2 days/year over the Larsen C ice shelf, 1.8 days/ year over the George VI ice shelf and 0.55 days/year over the Wilkins ice shelf area. The correlation between MI values and December-January (DJ) averaged air/surface temperature over selected locations show values ranging between similar to 0.8 and similar to 0.4. Results suggest that a 1 degrees C increase in the monthly averaged DJ air/surface temperature corresponds to an average MI increase of approximately 2.10(6) x km(2) x day. (C) 2009 Elsevier Inc. All rights reserved. C1 [Tedesco, M.] CUNY City Coll, Dept EAS, New York, NY 10031 USA. [Tedesco, M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Tedesco, M.] Univ Maryland, Baltimore, MD 21201 USA. RP Tedesco, M (reprint author), CUNY City Coll, Dept EAS, Marshak Bldg,Room J 106,138th St & Convent Av, New York, NY 10031 USA. EM mtedesco@sci.ccny.cuny.edu RI Tedesco, Marco/F-7986-2015 FU City University of New York; NASA; University of Maryland, Baltimore County [1253 10140 022 00002322, 1253 10140 022 00002264, 1253 10140 02200002262]; CUNY [93333-0001] FX This work was Supported by the City University of New York, NASA and the University of Maryland, Baltimore County through the grants UMBC 1253 10140 022 00002322, 1253 10140 022 00002264 and 1253 10140 02200002262 and CUNY 93333-0001. NR 25 TC 28 Z9 33 U1 0 U2 15 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 MAY 15 PY 2009 VL 113 IS 5 BP 979 EP 997 DI 10.1016/j.rse.2009.01.009 PG 19 WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic Technology SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science & Photographic Technology GA 440QY UT WOS:000265716000010 ER PT J AU Ivins, ER AF Ivins, Erik R. TI Ice Sheet Stability and Sea Level SO SCIENCE LA English DT Editorial Material ID ANTARCTICA; RISE C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Ivins, ER (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM eri@fryxell.jpl.nasa.gov NR 18 TC 7 Z9 7 U1 0 U2 2 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 MAY 15 PY 2009 VL 324 IS 5929 BP 888 EP 889 DI 10.1126/science.1173958 PG 2 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 445KD UT WOS:000266048800021 PM 19443771 ER PT J AU Zebker, HA Stiles, B Hensley, S Lorenz, R Kirk, RL Lunine, J AF Zebker, Howard A. Stiles, Bryan Hensley, Scott Lorenz, Ralph Kirk, Randolph L. Lunine, Jonathan TI Size and Shape of Saturn's Moon Titan SO SCIENCE LA English DT Article ID RADAR; ORIGIN; PLANETS; LAKES AB Cassini observations show that Saturn's moon Titan is slightly oblate. A fourth-order spherical harmonic expansion yields north polar, south polar, and mean equatorial radii of 2574.32 +/- 0.05 kilometers (km), 2574.36 +/- 0.03 km, and 2574.91 +/- 0.11 km, respectively; its mean radius is 2574.73 +/- 0.09 km. Titan's shape approximates a hydrostatic, synchronously rotating triaxial ellipsoid but is best fit by such a body orbiting closer to Saturn than Titan presently does. Titan's lack of high relief implies that most-but not all-of the surface features observed with the Cassini imaging subsystem and synthetic aperture radar are uncorrelated with topography and elevation. Titan's depressed polar radii suggest that a constant geopotential hydrocarbon table could explain the confinement of the hydrocarbon lakes to high latitudes. C1 [Zebker, Howard A.] Stanford Univ, Dept Geophys, Stanford, CA 94305 USA. [Zebker, Howard A.] Stanford Univ, Dept Elect Engn, Stanford, CA 94305 USA. [Stiles, Bryan; Hensley, Scott] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Lorenz, Ralph] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA. [Kirk, Randolph L.] US Geol Survey, Flagstaff, AZ 86001 USA. [Lunine, Jonathan] Univ Arizona, Dept Planetary Sci, Tucson, AZ 85721 USA. [Lunine, Jonathan] Univ Arizona, Dept Phys, Tucson, AZ 85721 USA. RP Zebker, HA (reprint author), Stanford Univ, Dept Geophys, Stanford, CA 94305 USA. EM zebker@stanford.edu RI Lorenz, Ralph/B-8759-2016 OI Lorenz, Ralph/0000-0001-8528-4644 FU Cassini Project; NASA FX We thank the Cassini Radar Team for detailed planning of these observations. This work was supported by the Cassini Project and by NASA as part of the Cassini Data Analysis Program. We also thank the reviewers for many constructive comments on our error analysis and data interpretation. The Cassini Project is a joint endeavor of NASA, the European Space Agency, and the Italian Space Agency. Cassini is managed by JPL, California Institute of Technology, under a contract with NASA. NR 19 TC 51 Z9 51 U1 0 U2 9 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 MAY 15 PY 2009 VL 324 IS 5929 BP 921 EP 923 DI 10.1126/science.1168905 PG 3 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 445KD UT WOS:000266048800033 PM 19342551 ER PT J AU Rind, D Lerner, J McLinden, C Perlwitz, J AF Rind, D. Lerner, J. McLinden, C. Perlwitz, J. TI Stratospheric ozone during the Last Glacial Maximum SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID CLIMATE; MODEL AB Stratospheric ozone during the Last Glacial Maximum (LGM) is investigated in on-line simulations with the GISS Global Climate/Middle Atmosphere Model 3. LGM boundary conditions and atmospheric concentrations are employed in three simulations: without interactive ozone, with ozone photochemistry appropriate for that time period and with the LGM climate but current atmospheric composition for chemistry. Results show stratospheric ozone increased during the LGM due to reduced NOy and chlorine, while warmer stratospheric temperatures (from reduced stratospheric CO(2)) decrease ozone with current photochemistry. The stratospheric residual circulation intensified in the lowermost stratosphere, increasing stratosphere/troposphere exchange at higher latitudes, although for most of the middle atmosphere the circulation decreased; the age of air in the Middle Atmosphere increased by up to one year. Compared with the vastly different LGM conditions, increase in stratospheric ozone of 2% by mass had little effect on atmospheric dynamics, and increased the global radiation balance by <0.1 Wm(-2). Citation: Rind, D., J. Lerner, C. McLinden, and J. Perlwitz (2009), Stratospheric ozone during the Last Glacial Maximum, Geophys. Res. Lett., 36, L09712, doi:10.1029/2009GL037617. C1 [Rind, D.; Perlwitz, J.] Columbia Univ, NASA, Goddard Inst Space Studies, New York, NY 10025 USA. [Lerner, J.] Columbia Univ, Ctr Climate Syst Res, New York, NY 10025 USA. [McLinden, C.] Environm Canada, Toronto, ON M3H 5T4, Canada. [Perlwitz, J.] Columbia Univ, Dept Appl Phys & Appl Math, New York, NY 10025 USA. RP Rind, D (reprint author), Columbia Univ, NASA, Goddard Inst Space Studies, 2880 Broadway, New York, NY 10025 USA. EM drind@giss.nasa.gov RI McLinden, Chris/A-7710-2010 OI McLinden, Chris/0000-0001-5054-1380 FU NASA FX We thank Jeff Jonas for help in setting up the LGM simulation. This work was supported by the NASA/Atmospheric composition focus area, while climate modeling at GISS is supported by the NASA Climate Change and Climate Variability focus area. The simulations were made with the support of the NASA HMD high speed computing program. NR 12 TC 5 Z9 5 U1 3 U2 7 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 MAY 14 PY 2009 VL 36 AR L09712 DI 10.1029/2009GL037617 PG 5 WC Geosciences, Multidisciplinary SC Geology GA 446CZ UT WOS:000266099300004 ER PT J AU Wu, DL Ackerman, SA Davies, R Diner, DJ Garay, MJ Kahn, BH Maddux, BC Moroney, CM Stephens, GL Veefkind, JP Vaughan, MA AF Wu, D. L. Ackerman, S. A. Davies, R. Diner, D. J. Garay, M. J. Kahn, B. H. Maddux, B. C. Moroney, C. M. Stephens, G. L. Veefkind, J. P. Vaughan, M. A. TI Vertical distributions and relationships of cloud occurrence frequency as observed by MISR, AIRS, MODIS, OMI, CALIPSO, and CloudSat SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID MULTIANGLE MEASUREMENTS; SPACEBORNE LIDAR; TOP HEIGHTS; PART I; RETRIEVAL; AEROSOLS; MISSION; RADAR AB Multi-sensor cloud height observations are investigated and compared in terms of vertical and latitudinal distributions of monthly mean cloud occurrence frequency (COF). Although this study emphasizes the standard Multiangle Imaging SpectroRadiometer (MISR) cloud top height (CTH) retrieval, the strengths and weakness among different passive and active remote sensing techniques with respect to cloud detection and height assessment are also discussed. The standard MISR CTH retrieval is less sensitive to high thin cirrus than the Atmospheric Infrared Sounder (AIRS) and Cloud-Aerosol Lidar and Infrared Pathfinder Satellite Observation (CALIPSO), but MISR provides more accurate CTH retrievals in the middle and lower troposphere compared with other passive sensors, especially for clouds in the planetary boundary layer. Citation: Wu, D. L., et al. (2009), Vertical distributions and relationships of cloud occurrence frequency as observed by MISR, AIRS, MODIS, OMI, CALIPSO, and CloudSat, Geophys. Res. Lett., 36, L09821, doi:10.1029/2009GL037464. C1 [Wu, D. L.; Diner, D. J.; Kahn, B. H.; Moroney, C. M.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Ackerman, S. A.; Maddux, B. C.] Univ Wisconsin, Dept Atmospher & Ocean Sci, Madison, WI 53706 USA. [Davies, R.] Univ Auckland, Dept Phys, Auckland 1020, New Zealand. [Garay, M. J.] Raytheon Corp, Intelligence & Informat Syst, Pasadena, CA 91101 USA. [Stephens, G. L.] Colorado State Univ, Dept Atmospher Sci, Ft Collins, CO 80523 USA. [Veefkind, J. P.] Royal Netherlands Meteorol Inst, Climate Res & Seismol Dept, NL-3730 AE De Bilt, Netherlands. [Vaughan, M. A.] NASA, Langley Res Ctr, Hampton, VA 23681 USA. RP Wu, DL (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM dong.l.wu@jpl.nasa.gov RI Davies, Roger/D-4296-2009; Ackerman, Steven/G-1640-2011; Wu, Dong/D-5375-2012 OI Davies, Roger/0000-0002-2991-0409; Ackerman, Steven/0000-0002-4476-0269; FU National Aeronautics and Space Administration (NASA) FX This work was performed at the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration (NASA). We would like to thank J.H. Jiang for providing CALIPSO reading code, and J. Blaisdell, Y. Hu, J. Joiner, R. Kahn, C. Trepte, and D. M. Winker for helpful discussions on AIRS, CALIPSO, MISR, and OMI data. GMAO efforts to provide the GEOS- 5.1 analysis and the data processing by the NASA Langley Research Center Atmospheric Sciences Data Center are gratefully acknowledged. NR 31 TC 29 Z9 29 U1 2 U2 19 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 MAY 14 PY 2009 VL 36 AR L09821 DI 10.1029/2009GL037464 PG 5 WC Geosciences, Multidisciplinary SC Geology GA 446CZ UT WOS:000266099300002 ER PT J AU Rind, D Jonas, J Stammerjohn, S Lonergan, P AF Rind, D. Jonas, J. Stammerjohn, S. Lonergan, P. TI The Antarctic ozone hole and the Northern Annular Mode: A stratospheric interhemispheric connection SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID HEMISPHERE CLIMATE-CHANGE; TEMPERATURE; SIMULATION; TRENDS AB The S.H. ozone hole deepened into the mid-1990s, while the Northern Annular Mode (NAM) became more positive. Both effects have since stabilized. We investigate a possible connection with modeling experiments of a S. H. spring ozone hole, and also year-round ozone loss in both polar regions. The S. H. ozone hole results in a more positive NAM-like phase extending down to the surface. Reduced vertical stability increases S. H. tropospheric wave energy flux into the stratosphere which drives a residual circulation with relative subsidence over the Southern pole and upwelling and reduced planetary wave energy flux at Northern high latitudes. The results suggest that similar trends in the Southern Ozone hole and the NAM over the last 20 years may be more than just a coincidence, although other factors undoubtedly influence the Northern high latitude circulation. Citation: Rind, D., J. Jonas, S. Stammerjohn, and P. Lonergan (2009), The Antarctic ozone hole and the Northern Annular Mode: A stratospheric interhemispheric connection, Geophys. Res. Lett., 36, L09818, doi: 10.1029/2009GL037866. C1 [Rind, D.; Stammerjohn, S.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA. [Jonas, J.; Lonergan, P.] Columbia Univ, Ctr Climate Syst Res, New York, NY 10025 USA. RP Rind, D (reprint author), NASA, Goddard Inst Space Studies, New York, NY 10025 USA. EM drind@giss.nasa.gov OI STAMMERJOHN, SHARON/0000-0002-1697-8244 FU NASA Atmospheric Composition Focus Area; NASA HMD high speed computing program FX This work was supported by the NASA Atmospheric Composition Focus Area and the NASA HMD high speed computing program. We also thank the referenced website for EP flux data. NR 22 TC 8 Z9 8 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 MAY 13 PY 2009 VL 36 AR L09818 DI 10.1029/2009GL037866 PG 5 WC Geosciences, Multidisciplinary SC Geology GA 446CX UT WOS:000266099100006 ER PT J AU Han, SC Kim, HJ Yeo, IY Yeh, P Oki, T Seo, KW Alsdorf, D Luthcke, SB AF Han, Shin-Chan Kim, Hyungjun Yeo, In-Young Yeh, Pat Oki, Taikan Seo, Ki-Weon Alsdorf, Doug Luthcke, Scott B. TI Dynamics of surface water storage in the Amazon inferred from measurements of inter-satellite distance change SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID RIVER; SYSTEM; BRAZIL; MODELS; SCALE; BASIN AB Terrestrial water storage in the Amazon basin and its surrounding areas is studied by exploring the instantaneous measurements of distance changes between two satellites from the GRACE mission. The surface water in the channels and floodplains can be significant in weighing total water storage. Its magnitude can be as large as soil moisture perturbing the motions of the satellites to a detectable amount by the on-board instrument. The river runoff routing simulations indicate the effective velocity throughout the Amazon basin over the years is about 30 cm/s with significant seasonal change. The lower velocity, during rising stages and peak water season, and the faster velocity, during falling stages, are delineated from the observations. The backwater effects may impact such seasonal change on the overall flow velocity. Direct assimilation of GRACE tracking data can contribute to land surface dynamic processes by resolving the time scale of transport in rivers and streams. Citation: Han, S.-C., H. Kim, I.-Y. Yeo, P. Yeh, T. Oki, K.-W. Seo, D. Alsdorf, and S. B. Luthcke (2009), Dynamics of surface water storage in the Amazon inferred from measurements of inter-satellite distance change, Geophys. Res. Lett., 36, L09403, doi:10.1029/2009GL037910. C1 [Han, Shin-Chan; Luthcke, Scott B.] NASA, Goddard Space Flight Ctr, Planetary Geodynam Lab, Greenbelt, MD 20771 USA. [Han, Shin-Chan] Univ Maryland Baltimore Cty, Goddard Earth Sci & Technol Ctr, Baltimore, MD 21228 USA. [Kim, Hyungjun; Yeh, Pat; Oki, Taikan] Univ Tokyo, Inst Ind Sci, Meguro Ku, Tokyo 1538505, Japan. [Yeo, In-Young] Univ Maryland, Dept Geog, College Pk, MD 20742 USA. [Seo, Ki-Weon] Korea Polar Res Inst, Inchon 911098099, South Korea. [Alsdorf, Doug] Ohio State Univ, Sch Earth Sci, Columbus, OH 43210 USA. RP Han, SC (reprint author), NASA, Goddard Space Flight Ctr, Planetary Geodynam Lab, Greenbelt, MD 20771 USA. EM shin-chan.han@nasa.gov RI Oki, Taikan/E-5778-2010; Luthcke, Scott/D-6283-2012; Han, Shin-Chan/A-2022-2009; YEH, Pat/B-2758-2011; KIM, HYUNGJUN/I-5099-2014 OI Oki, Taikan/0000-0003-4067-4678; YEH, Pat/0000-0001-7629-3362; KIM, HYUNGJUN/0000-0003-1083-8416 NR 14 TC 25 Z9 25 U1 0 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 MAY 12 PY 2009 VL 36 AR L09403 DI 10.1029/2009GL037910 PG 5 WC Geosciences, Multidisciplinary SC Geology GA 446CW UT WOS:000266099000006 ER PT J AU Slavin, JA Acuna, MH Anderson, BJ Barabash, S Benna, M Boardsen, SA Fraenz, M Gloeckler, G Gold, RE Ho, GC Korth, H Krimigis, SM McNutt, RL Raines, JM Sarantos, M Solomon, SC Zhang, T Zurbuchen, TH AF Slavin, James A. Acuna, Mario H. Anderson, Brian J. Barabash, Stas Benna, Mehdi Boardsen, Scott A. Fraenz, Markus Gloeckler, George Gold, Robert E. Ho, George C. Korth, Haje Krimigis, Stamatios M. McNutt, Ralph L., Jr. Raines, Jim M. Sarantos, Menelaos Solomon, Sean C. Zhang, Tielong Zurbuchen, Thomas H. TI MESSENGER and Venus Express observations of the solar wind interaction with Venus SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID MAGNETIC-FIELD; BOW SHOCK; MAGNETOTAIL; LOCATION AB At 23: 08 UTC on 5 June 2007 the MESSENGER spacecraft reached its closest approach altitude of 338 km during its final flyby of Venus en route to its 2011 orbit insertion at Mercury. The availability of the simultaneous Venus Express solar wind and interplanetary magnetic field measurements provides a rare opportunity to examine the influence of upstream conditions on this planet's solar wind interaction. We present MESSENGER observations of new features of the Venus - solar wind interaction including hot flow anomalies upstream of the bow shock, a flux rope in the near-tail and a two-point determination of the timescale for magnetic flux transport through this induced magnetosphere. Citation: Slavin, J. A., et al. (2009), MESSENGER and Venus Express observations of the solar wind interaction with Venus, Geophys. Res. Lett., 36, L09106, doi:10.1029/2009GL037876. C1 [Slavin, James A.; Boardsen, Scott A.; Sarantos, Menelaos] NASA, Goddard Space Flight Ctr, Heliophys Sci Div, Greenbelt, MD 20771 USA. [Acuna, Mario H.; Benna, Mehdi] NASA, Goddard Space Flight Ctr, Solar Syst Explorat Div, Greenbelt, MD 20771 USA. [Anderson, Brian J.; Gold, Robert E.; Ho, George C.; Korth, Haje; Krimigis, Stamatios M.; McNutt, Ralph L., Jr.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA. [Barabash, Stas] Swedish Inst Space Phys, SE-98128 Kiruna, Sweden. [Fraenz, Markus] Max Planck Inst Solar Syst Res, D-37191 Katlenburg Lindau, Germany. [Gloeckler, George; Raines, Jim M.; Zurbuchen, Thomas H.] Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA. [Zhang, Tielong] Austrian Acad Sci, Space Res Inst, A-8042 Graz, Austria. [Solomon, Sean C.] Carnegie Inst Washington, Dept Terr Magnetism, Washington, DC 20015 USA. RP Slavin, JA (reprint author), NASA, Goddard Space Flight Ctr, Heliophys Sci Div, Code 670, Greenbelt, MD 20771 USA. EM james.a.slavin@nasa.gov RI McNutt, Ralph/E-8006-2010; Anderson, Brian/I-8615-2012; Slavin, James/H-3170-2012; Sarantos, Menelaos/H-8136-2013; Ho, George/G-3650-2015; Benna, Mehdi/F-3489-2012 OI McNutt, Ralph/0000-0002-4722-9166; Slavin, James/0000-0002-9206-724X; Ho, George/0000-0003-1093-2066; FU NASA [NASW-00002]; Carnegie Institution of Washington [NAS5-97271]; Johns Hopkins University Applied Physics Laboratory FX Computational assistance and data visualization support provided by C. Liebrecht are gratefully acknowledged. The MESSENGER project is supported by the NASA Discovery Program under contracts NASW-00002 to the Carnegie Institution of Washington and NAS5-97271 to the Johns Hopkins University Applied Physics Laboratory. NR 21 TC 16 Z9 16 U1 1 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 MAY 12 PY 2009 VL 36 AR L09106 DI 10.1029/2009GL037876 PG 6 WC Geosciences, Multidisciplinary SC Geology GA 446CW UT WOS:000266099000005 ER PT J AU Su, H Jiang, JH Stephens, GL Vane, DG Livesey, NJ AF Su, Hui Jiang, Jonathan H. Stephens, Graeme L. Vane, Deborah G. Livesey, Nathaniel J. TI Radiative effects of upper tropospheric clouds observed by Aura MLS and CloudSat SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID CIRRUS CLOUDS; PARAMETERIZATION AB The radiative effects of upper tropospheric (UT) clouds observed by CloudSat and Aura MLS during June-JulyAugust 2008 are examined and contrasted. We find that the UT cloud occurrence frequency observed by MLS is more than CloudSat by 4-10% in the tropical average and by 40 similar to 60% near the tropopause in the deep convective regions. The clouds detected by MLS but missed by CloudSat (denoted as TCC) typically have visible optical thickness less than 0.2. TCC produce a tropical-mean net warming of 3.5 W/m(2) at the top-of-atmosphere and net cooling of 1.2 W/m(2) at the surface. They induce a net radiative heating in the UT. Their heating rate at 200 hPa is similar to 0.35 K/day in the tropical-mean and similar to 0.8 K/day over South Asia, which is about 3-4 times the clear-sky radiative heating rate. Hence, they are potentially important in affecting the mass transport rates from the troposphere to the stratosphere. Citation: Su, H., J. H. Jiang, G. L. Stephens, D. G. Vane, and N. J. Livesey (2009), Radiative effects of upper tropospheric clouds observed by Aura MLS and CloudSat, Geophys. Res. Lett., 36, L09815, doi:10.1029/2009GL037173. C1 [Su, Hui; Jiang, Jonathan H.; Vane, Deborah G.; Livesey, Nathaniel J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Stephens, Graeme L.] Colorado State Univ, Dept Atmospher Sci, Ft Collins, CO 80523 USA. RP Su, H (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM hui.su@jpl.nasa.gov FU JPL R&TD and NASA ROSES ACMAP-AST FX We thank the funding support from the JPL R&TD and NASA ROSES ACMAP-AST program. We thank Tristan L'Ecuyer for help with CloudSat data, Yu Gu for help with the Fu-Liou radiative transfer modeling, and two anonymous reviewers for helpful comments. This work is conducted at the Jet Propulsion Laboratory, California Institute of Technology, under contract with NASA. NR 14 TC 14 Z9 14 U1 0 U2 4 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 EI 1944-8007 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD MAY 12 PY 2009 VL 36 AR L09815 DI 10.1029/2009GL037173 PG 5 WC Geosciences, Multidisciplinary SC Geology GA 446CW UT WOS:000266099000001 ER PT J AU Weber, RC Bills, BG Johnson, CL AF Weber, R. C. Bills, B. G. Johnson, C. L. TI Constraints on deep moonquake focal mechanisms through analyses of tidal stress SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Article ID FOCUS EARTHQUAKES; LUNAR SEISMICITY; MOON; TECTONICS; MANTLE; MODEL AB A relationship between deep moonquake occurrence and tidal forcing is suggested by the monthly periodicities observed in the occurrence times of events recorded by the Apollo Passive Seismic Experiment. In addition, the typically large S wave to P wave arrival amplitude ratios observed on deep moonquake seismograms are indicative of shear failure. Tidal stress, induced in the lunar interior by the gravitational influence of the Earth, may influence moonquake activity. We investigate the relationship between tidal stress and deep moonquake occurrence by searching for a linear combination of the normal and shear components of tidal stress that best approximates a constant value when evaluated at the times of moonquakes from 39 different moonquake clusters. We perform a grid search at each cluster location, computing the stresses resolved onto a suite of possible failure planes, to obtain the best fitting fault orientation at each location. We find that while linear combinations of stresses (and in some cases stress rates) can fit moonquake occurrence at many clusters quite well; for other clusters, the fit is not strongly dependent on plane orientation. This suggests that deep moonquakes may occur in response to factors other than, or in addition to, tidal stress. Several of our inferences support the hypothesis that deep moonquakes might be related to transformational faulting, in which shear failure is induced by mineral phase changes at depth. The occurrence of this process would have important implications for the lunar interior. C1 [Weber, R. C.] US Geol Survey, Flagstaff, AZ 86001 USA. [Bills, B. G.; Johnson, C. L.] Univ Calif San Diego, Scripps Inst Oceanog, Cecil H & Ida M Green Inst Geophys & Planetary Ph, La Jolla, CA 92093 USA. [Bills, B. G.] NASA, Jet Prop Lab, Pasadena, CA USA. [Johnson, C. L.] Univ British Columbia, Dept Earth & Ocean Sci, Vancouver, BC V5Z 1M9, Canada. RP Weber, RC (reprint author), US Geol Survey, 2255 N Gemini Dr, Flagstaff, AZ 86001 USA. EM rweber@usgs.gov FU Eugene M. Shoemaker Planetary Geology and Geophysics Fellowship; NSERC; [NASA-NNG05GK34G]; [NASA-NNX08AL49G] FX The authors would like to thank Justin Hagerty, Robin Fergason, Yosio Nakamura, Cliff Frohlich, and an anonymous reviewer for their thoughtful comments on this manuscript. This work was supported by the Eugene M. Shoemaker Planetary Geology and Geophysics Fellowship awarded to R. C. W., and grants NASA-NNG05GK34G, NASA-NNX08AL49G, and NSERC to C. L. J. NR 43 TC 12 Z9 13 U1 0 U2 4 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 MAY 12 PY 2009 VL 114 AR E05001 DI 10.1029/2008JE003286 PG 17 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 446DU UT WOS:000266101400001 ER PT J AU Nose, M Taguchi, S Christon, SP Collier, MR Moore, TE Carlson, CW McFadden, JP AF Nose, M. Taguchi, S. Christon, S. P. Collier, M. R. Moore, T. E. Carlson, C. W. McFadden, J. P. TI Response of ions of ionospheric origin to storm time substorms: Coordinated observations over the ionosphere and in the plasma sheet SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article ID MASS-SPECTROMETER OBSERVATIONS; NEAR-EARTH MAGNETOTAIL; MAGNETOSPHERIC PLASMA; MAGNETIC ACTIVITY; EXPANSION PHASE; DE-1 ALTITUDES; OUTFLOW; WIND; DISTRIBUTIONS; MISSION AB We investigate variations of ion flux over the ionosphere and in the plasma sheet when storm time substorms are initiated, using simultaneous observations of neutral atoms in the energy range of up to a few keV measured by the low-energy neutral atom (LENA) imager on board the Imager for Magnetopause-to-Aurora Global Exploration ( IMAGE) satellite, outflowing ion flux of <1 keV measured by the ion electrostatic analyzer (IESA) on board the Fast Auroral SnapshoT (FAST) satellite, and energetic (9-210 keV/e) ion flux measured by the energetic particle and ion composition (EPIC) instrument on board the Geotail satellite. We examined three storm intervals during which the IMAGE or FAST satellite was in a suitable location to observe ionospheric ion outflow and the Geotail satellite was in the plasma sheet on the nightside. The neutral atom flux observed by IMAGE/LENA in the first interval and outflowing ion flux observed by FAST/IESA in the second and third intervals indicate that storm time substorms can cause increases of low-energy ion flux over the ionosphere by a factor of 3-50 with time delay of less than several minutes. In the plasma sheet, the flux ratio of O+/H+ is rapidly enhanced at the storm time substorms and then increased gradually or stayed at a constant level in a time scale of similar to 1 h, suggesting a mass-dependent acceleration of ions at local dipolarization and a subsequent additional supply of O+ ions to the plasma sheet which have been extracted from the ionosphere at the substorms. These coordinated observations revealed that substorms have both an immediate effect and a delayed effect (i.e., two-step effect) on the ion composition in the plasma sheet. C1 [Nose, M.] Kyoto Univ, Data Anal Ctr Geomagnetism & Space Magnetism, Grad Sch Sci, Sakyo Ku, Kyoto 6068502, Japan. [Taguchi, S.] Univ Electrocommun, Dept Informat & Commun Engn, Tokyo 1828585, Japan. [Christon, S. P.] Focused Anal & Res, Columbia, MD 21044 USA. [Collier, M. R.; Moore, T. E.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Carlson, C. W.; McFadden, J. P.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. RP Nose, M (reprint author), Kyoto Univ, Data Anal Ctr Geomagnetism & Space Magnetism, Grad Sch Sci, Sakyo Ku, Oiwake Cho, Kyoto 6068502, Japan. EM nose@kugi.kyoto-u.ac.jp RI Moore, Thomas/D-4675-2012; Collier, Michael/I-4864-2013; Nose, Masahito/B-1900-2015; OI Moore, Thomas/0000-0002-3150-1137; Collier, Michael/0000-0001-9658-6605; Nose, Masahito/0000-0002-2789-3588; Christon, Stephen/0000-0003-1770-2458 FU Kurata Memorial Hitachi Science and Technology Foundation [844]; Japan Securities Scholarship Foundation [1368]; Inamori Foundation; Ministry of Education, Science, Sports and Culture [17740327, 19740303] FX We thank D. J. Williams, R. W. McEntire, A. T. Y. Lui, and S. R. Nylund for their help in processing the Geotail/EPIC data. We also thank T. Nagai for providing the Geotail/MGF data. The geomagnetic field data from high-latitude stations (LER, NAQ, GLN, and BLC) were provided by institutes operating each station through INTERMAGNET and WDC for Geomagnetism, Kyoto. The SYM-H index was provided by T. Iyemori at WDC for Geomagnetism, Kyoto. The GOES 10 magnetic field data were provided by H. Singer through the NOAA/NGDC SPIDR (Space Physics Interactive Data Resource) Web site. The energetic particle data from the LANL geosynchronous satellites were provided by courtesy of G. Reeves and D. Belian. Thanks are due to K. Hosowaka, Y. Miyashita, Y. Ogawa, and A. Ieda for their helpful comments. This work was supported by the Kurata Memorial Hitachi Science and Technology Foundation (grant 844), the Japan Securities Scholarship Foundation (grant 1368), Inamori Foundation, and the Ministry of Education, Science, Sports and Culture, Grant-in-Aid for Young Scientists (B) (grants 17740327 and 19740303).; [35] Wolfgang Baumjohann thanks Dimitrios Sarafopoulos and another reviewer for their assistance in evaluating this paper. NR 50 TC 14 Z9 14 U1 0 U2 2 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 MAY 12 PY 2009 VL 114 AR A05207 DI 10.1029/2009JA014048 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 446ED UT WOS:000266102400002 ER PT J AU Nugent, PW Shaw, JA Piazzolla, S AF Nugent, Paul W. Shaw, Joseph A. Piazzolla, Sabino TI Infrared cloud imaging in support of Earth-space optical communication SO OPTICS EXPRESS LA English DT Article ID CALIBRATION; STATISTICS; LINK AB The increasing need for high data return from near-Earth and deep-space missions is driving a demand for the establishment of Earth-space optical communication links. These links will require a nearly obstruction-free path to the communication platform, so there is a need to measure spatial and temporal statistics of clouds at potential ground-station sites. A technique is described that uses a ground-based thermal infrared imager to provide continuous day-night cloud detection and classification according to the cloud optical depth and potential communication channel attenuation. The benefit of retrieving cloud optical depth and corresponding attenuation is illustrated through measurements that identify cloudy times when optical communication may still be possible through thin clouds. (C) 2009 Optical Society of America C1 [Nugent, Paul W.; Shaw, Joseph A.] Montana State Univ, Dept Elect & Comp Engn, Bozeman, MT 59717 USA. [Piazzolla, Sabino] CALTECH, Jet Prop Lab, Opt Commun Grp, Pasadena, CA 91109 USA. RP Shaw, JA (reprint author), Montana State Univ, Dept Elect & Comp Engn, Bozeman, MT 59717 USA. EM jshaw@montana.edu FU NASA Stennis Space Center FX We gratefully acknowledge financial support provided by a Graduate Student Research Program fellowship through the NASA Stennis Space Center and use of a thermal chamber at the Montana State University Space Science and Engineering Laboratory. NR 18 TC 22 Z9 22 U1 1 U2 1 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 MAY 11 PY 2009 VL 17 IS 10 BP 7862 EP 7872 PG 11 WC Optics SC Optics GA 450DT UT WOS:000266381900016 PM 19434118 ER PT J AU Bockelee-Morvan, D Woodward, CE Kelley, MS Wooden, DH AF Bockelee-Morvan, Dominique Woodward, Charles E. Kelley, Michael S. Wooden, Diane H. TI WATER IN COMETS 71P/CLARK AND C/2004 B1 (LINEAR) WITH SPITZER SO ASTROPHYSICAL JOURNAL LA English DT Article DE comets: individual (71P/Clark, C/2004 B1 LINEAR); infrared: solar system ID SPIN TEMPERATURES; SPACE-TELESCOPE; DEEP IMPACT; DUST; TEMPEL-1; SPECTRUM; EJECTA; O1 AB We present 5.5-7.6 mu m spectra of comets 71P/Clark (2006 May 27.56 UT, r(h) = 1.57 AU pre-perihelion) and C/2004 B1 (LINEAR) (2005 October 15.22 UT, r(h) = 2.21 AU pre-perihelion and 2006 May 16.22 UT, r(h) = 2.06 AU post-perihelion) obtained with the Spitzer Space Telescope. The nu(2) vibrational band of water is detected with a signal-to-noise ratio of 11-50. Fitting the spectra using a fluorescence model of water emission yields a water rotational temperature of < 18 K for 71P/Clark and similar or equal to 14 +/- 2K (pre-perihelion) and 23 +/- 4K (post-perihelion) for C/2004 B1 (LINEAR). The water ortho-to-para ratio in C/2004 B1 (LINEAR) is measured to be 2.31 +/- 0.18, which corresponds to a spin temperature of 26(-2)(+3) K. Water production rates are derived. The agreement between the water model and the measurements is good, as previously found for Spitzer spectra of C/2003 K4 (LINEAR). The Spitzer spectra of these three comets do not show any evidence for emission from polycyclic aromatic hydrocarbons and carbonate minerals, in contrast to results reported for comets 9P/Tempel 1 and C/1995 O1 (Hale-Bopp). C1 [Bockelee-Morvan, Dominique] Observ Paris, LESIA, F-92195 Meudon, France. [Woodward, Charles E.] Univ Minnesota, Sch Phys & Astron, Dept Astron, Minneapolis, MN 55455 USA. [Kelley, Michael S.] Univ Cent Florida, Dept Phys, Orlando, FL 32816 USA. [Wooden, Diane H.] NASA, Ames Res Ctr, Moffett Field, CA 94305 USA. RP Bockelee-Morvan, D (reprint author), Observ Paris, LESIA, 5 Pl Jules Janssen, F-92195 Meudon, France. EM dominique.bockelee@obspm.fr; chelsea@astro.umn.edu; msk@astro.umd.edu; d.h.wooden@nasa.gov OI Kelley, Michael/0000-0002-6702-7676 FU NASA [1263741, 1256406, 1215746]; National Science Foundation [AST-0706980] FX This work is based on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology under a contract with NASA. Support for this work was provided by NASA through an award issued by JPL/Caltech. Support for this work was also provided by NASA through contracts 1263741, 1256406, and 1215746 issued by JPL/Caltech to the University of Minnesota. C. E. W. also acknowledges support from the National Science Foundation grant AST-0706980. We thank the anonymous referee for helpful comments, and N. Biver, D. E. Harker and D. Pelat for enlightening discussions. NR 43 TC 13 Z9 13 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAY 10 PY 2009 VL 696 IS 2 BP 1075 EP 1083 DI 10.1088/0004-637X/696/2/1075 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 441IO UT WOS:000265762700002 ER PT J AU Abdo, AA Ackermann, M Atwood, WB Bagagli, R Baldini, L Ballet, J Band, DL Barbiellini, G Baring, MG Bartelt, J Bastieri, D Baughman, BM Bechtol, K Bellardi, F Bellazzini, R Berenji, B Bisello, D Blandford, RD Bloom, ED Bogart, JR Bonamente, E Borgland, AW Bouvier, A Bregeon, J Brez, A Brigida, M Bruel, P Burnett, TH Caliandro, GA Cameron, RA Camilo, F Caraveo, PA Casandjian, JM Ceccanti, M Cecchi, C Charles, E Chekhtman, A Cheung, CC Chiang, J Ciprini, S Claus, R Cognard, I Cohen-Tanugi, J Cominsky, LR Conrad, J Corbet, R Corucci, L Cutini, S Davis, DS DeKlotz, M Dermer, CD de Angelis, A de Palma, F Digel, SW Dormody, M Silva, EDE Drell, PS Dubois, R Dumora, D Espinoza, C Farnier, C Favuzzi, C Flath, DL Fleury, P Focke, WB Frailis, M Friere, PCC Fukazawa, Y Funk, S Fusco, P Gargano, F Gasparrini, D Gehrels, N Germani, S Giannitrapani, R Giebels, B Giglietto, N Giordano, F Glanzman, T Godfrey, G Gotthelf, EV Grenier, IA Grondin, MH Grove, JE Guillemot, L Guiriec, S Haller, G Harding, AK Hart, PA Hartman, RC Hays, E Hobbs, G Hughes, RE Johannesson, G Johnson, AS Johnson, RP Johnson, TJ Johnson, WN Johnston, S Kamae, T Kanbach, G Kaspi, VM Katagiri, H Kataoka, J Kavelaars, A Kawai, N Kelly, H Kerr, M Kiziltan, B Klamra, W Knodlseder, J Kramer, M Kuehn, F Kuss, M Lande, J Landriu, D Latronico, L Lee, B Lee, SH Lemoine-Goumard, M Livingstone, M Longo, F Loparco, F Lott, B Lovellette, MN Lubrano, P Lyne, AG Madejski, GM Makeev, A Manchester, RN Marangelli, B Marelli, M Mazziotta, MN McEnery, JE McGlynn, S McLaughlin, MA Menon, N Meurer, C Michelson, PF Mineo, T Mirizzi, N Mitthumsiri, W Mizuno, T Moiseev, AA Mongelli, M Monte, C Monzani, ME Moretti, E Morselli, A Moskalenko, IV Murgia, S Nakamori, T Nolan, PL Noutsos, A Nuss, E Ohsugi, T Omodei, N Orlando, E Ormes, JF Ozaki, M Paccagnella, A Paneque, D Panetta, JH Parent, D Pearce, M Pepe, M Perchiazzi, M Pesce-Rollins, M Pieri, L Pinchera, M Piron, F Porter, TA Raino, S Rando, R Ransom, SM Rapposelli, E Razzano, M Reimer, A Reimer, O Reposeur, T Reyes, LC Ritz, S Rochester, LS Rodriguez, AY Romani, RW Roth, M Ryde, F Sacchetti, A Sadrozinski, HFW Saggini, N Sanchez, D Sander, A Parkinson, PMS Segal, KN Sellerholm, A Sgro, C Siskind, EJ Smith, DA Smith, PD Spandre, G Spinelli, P Stamatikos, M Starck, JL Stecker, FW Stephens, TE Strickman, MS Strong, AW Suson, DJ Tajima, H Takahashi, H Takahashi, T Tanaka, T Tenze, A Thayer, JB Thayer, JG Theureau, G Thompson, DJ Thorsett, SE Tibaldo, L Tibolla, O Torres, DF Tramacere, A Turri, M Usher, TL Vigiani, L Vilchez, N Vitale, V Waite, AP Wang, P Watters, K Weltevrede, P Winer, BL Wood, KS Ylinen, T Ziegler, M AF Abdo, A. A. Ackermann, M. Atwood, W. B. Bagagli, R. Baldini, L. Ballet, J. Band, D. L. Barbiellini, G. Baring, M. G. Bartelt, J. Bastieri, D. Baughman, B. M. Bechtol, K. Bellardi, F. Bellazzini, R. Berenji, B. Bisello, D. Blandford, R. D. Bloom, E. D. Bogart, J. R. Bonamente, E. Borgland, A. W. Bouvier, A. Bregeon, J. Brez, A. Brigida, M. Bruel, P. Burnett, T. H. Caliandro, G. A. Cameron, R. A. Camilo, F. Caraveo, P. A. Casandjian, J. M. Ceccanti, M. Cecchi, C. Charles, E. Chekhtman, A. Cheung, C. C. Chiang, J. Ciprini, S. Claus, R. Cognard, I. Cohen-Tanugi, J. Cominsky, L. R. Conrad, J. Corbet, R. Corucci, L. Cutini, S. Davis, D. S. DeKlotz, M. Dermer, C. D. de Angelis, A. de Palma, F. Digel, S. W. Dormody, M. do Couto e Silva, E. Drell, P. S. Dubois, R. Dumora, D. Espinoza, C. Farnier, C. Favuzzi, C. Flath, D. L. Fleury, P. Focke, W. B. Frailis, M. Friere, P. C. C. Fukazawa, Y. Funk, S. Fusco, P. Gargano, F. Gasparrini, D. Gehrels, N. Germani, S. Giannitrapani, R. Giebels, B. Giglietto, N. Giordano, F. Glanzman, T. Godfrey, G. Gotthelf, E. V. Grenier, I. A. Grondin, M. -H. Grove, J. E. Guillemot, L. Guiriec, S. Haller, G. Harding, A. K. Hart, P. A. Hartman, R. C. Hays, E. Hobbs, G. Hughes, R. E. Johannesson, G. Johnson, A. S. Johnson, R. P. Johnson, T. J. Johnson, W. N. Johnston, S. Kamae, T. Kanbach, G. Kaspi, V. M. Katagiri, H. Kataoka, J. Kavelaars, A. Kawai, N. Kelly, H. Kerr, M. Kiziltan, B. Klamra, W. Knodlseder, J. Kramer, M. Kuehn, F. Kuss, M. Lande, J. Landriu, D. Latronico, L. Lee, B. Lee, S. -H. Lemoine-Goumard, M. Livingstone, M. Longo, F. Loparco, F. Lott, B. Lovellette, M. N. Lubrano, P. Lyne, A. G. Madejski, G. M. Makeev, A. Manchester, R. N. Marangelli, B. Marelli, M. Mazziotta, M. N. McEnery, J. E. McGlynn, S. McLaughlin, M. A. Menon, N. Meurer, C. Michelson, P. F. Mineo, T. Mirizzi, N. Mitthumsiri, W. Mizuno, T. Moiseev, A. A. Mongelli, M. Monte, C. Monzani, M. E. Moretti, E. Morselli, A. Moskalenko, I. V. Murgia, S. Nakamori, T. Nolan, P. L. Noutsos, A. Nuss, E. Ohsugi, T. Omodei, N. Orlando, E. Ormes, J. F. Ozaki, M. Paccagnella, A. Paneque, D. Panetta, J. H. Parent, D. Pearce, M. Pepe, M. Perchiazzi, M. Pesce-Rollins, M. Pieri, L. Pinchera, M. Piron, F. Porter, T. A. Raino, S. Rando, R. Ransom, S. M. Rapposelli, E. Razzano, M. Reimer, A. Reimer, O. Reposeur, T. Reyes, L. C. Ritz, S. Rochester, L. S. Rodriguez, A. Y. Romani, R. W. Roth, M. Ryde, F. Sacchetti, A. Sadrozinski, H. F. -W. Saggini, N. Sanchez, D. Sander, A. Parkinson, P. M. Saz Segal, K. N. Sellerholm, A. Sgro, C. Siskind, E. J. Smith, D. A. Smith, P. D. Spandre, G. Spinelli, P. Stamatikos, M. Starck, J. -L. Stecker, F. W. Stephens, T. E. Strickman, M. S. Strong, A. W. Suson, D. J. Tajima, H. Takahashi, H. Takahashi, T. Tanaka, T. Tenze, A. Thayer, J. B. Thayer, J. G. Theureau, G. Thompson, D. J. Thorsett, S. E. Tibaldo, L. Tibolla, O. Torres, D. F. Tramacere, A. Turri, M. Usher, T. L. Vigiani, L. Vilchez, N. Vitale, V. Waite, A. P. Wang, P. Watters, K. Weltevrede, P. Winer, B. L. Wood, K. S. Ylinen, T. Ziegler, M. TI FERMI LARGE AREA TELESCOPE OBSERVATIONS OF THE VELA PULSAR SO ASTROPHYSICAL JOURNAL LA English DT Article DE gamma rays: observations; pulsars: individual (PSR B0833-45) ID GAMMA-RAY PULSARS; POLAR-CAP; TIMING PACKAGE; LIGHT CURVES; SLOT GAPS; EMISSION; RADIATION; MODEL; MAGNETOSPHERES; DISCOVERY AB The Vela pulsar is the brightest persistent source in the GeV sky and thus is the traditional first target for new gamma-ray observatories. We report here on initial Fermi Large Area Telescope observations during verification phase pointed exposure and early sky survey scanning. We have used the Vela signal to verify Fermi timing and angular resolution. The high-quality pulse profile, with some 32,400 pulsed photons at E >= 0.03 GeV, shows new features, including pulse structure as fine as 0.3 ms and a distinct third peak, which shifts in phase with energy. We examine the high-energy behavior of the pulsed emission; initial spectra suggest a phase-averaged power-law index of Gamma = 1.51(-0.04)(+0.05) with an exponential cutoff at E-c = 2.9 +/- 0.1 GeV. Spectral fits with generalized cutoffs of the form e(-(E/Ec)b) require b <= 1, which is inconsistent with magnetic pair attenuation, and thus favor outer-magnetosphere emission models. Finally, we report on upper limits to any unpulsed component, as might be associated with a surrounding pulsar wind nebula. C1 [Abdo, A. A.; Dermer, C. D.; Grove, J. E.; Johnson, W. N.; Lovellette, M. N.; Strickman, M. S.; Wood, K. S.] USN, Res Lab, Div Space Sci, Washington, DC 20375 USA. [Ackermann, M.; Bartelt, J.; Bechtol, K.; Berenji, B.; Blandford, R. D.; Bloom, E. D.; Bogart, J. R.; Borgland, A. W.; Bouvier, A.; Cameron, R. A.; Charles, E.; Chiang, J.; Claus, R.; Digel, S. W.; do Couto e Silva, E.; Drell, P. S.; Dubois, R.; Flath, D. L.; Focke, W. B.; Funk, S.; Glanzman, T.; Godfrey, G.; Haller, G.; Hart, P. A.; Johannesson, G.; Johnson, A. S.; Kamae, T.; Kavelaars, A.; Kelly, H.; Lee, S. -H.; Madejski, G. M.; Mitthumsiri, W.; Monzani, M. E.; Moskalenko, I. V.; Murgia, S.; Nolan, P. L.; Paneque, D.; Panetta, J. H.; Reimer, A.; Reimer, O.; Rochester, L. S.; Romani, R. W.; Tajima, H.; Tanaka, T.; Thayer, J. B.; Thayer, J. G.; Waite, A. P.; Wang, P.; Watters, K.] Stanford Univ, Dept Phys, Kavli Inst Particle Astrophys & Cosmol, WW Hansen Expt Phys Lab, Stanford, CA 94305 USA. [Ackermann, M.; Bartelt, J.; Bechtol, K.; Berenji, B.; Blandford, R. D.; Bloom, E. D.; Bogart, J. R.; Borgland, A. W.; Bouvier, A.; Cameron, R. A.; Charles, E.; Chiang, J.; Claus, R.; Digel, S. W.; do Couto e Silva, E.; Drell, P. S.; Dubois, R.; Focke, W. B.; Funk, S.; Godfrey, G.; Haller, G.; Hart, P. A.; Johannesson, G.; Johnson, A. S.; Kamae, T.; Kavelaars, A.; Kelly, H.; Lee, S. -H.; Madejski, G. M.; Mitthumsiri, W.; Murgia, S.; Nolan, P. L.; Paneque, D.; Panetta, J. H.; Reimer, A.; Reimer, O.; Rochester, L. S.; Romani, R. W.; Tajima, H.; Tanaka, T.; Thayer, J. B.; Thayer, J. G.; Turri, M.; Usher, T. L.; Waite, A. P.; Wang, P.; Watters, K.] Stanford Univ, Stanford Linear Accelerator Ctr, Stanford, CA 94305 USA. [Atwood, W. B.; Porter, T. A.; Sadrozinski, H. F. -W.; Parkinson, P. M. Saz; Thorsett, S. E.; Ziegler, M.] Univ Calif Santa Cruz, Dept Phys, Santa Cruz Inst Particle Phys, Santa Cruz, CA 95064 USA. [Atwood, W. B.; Porter, T. A.; Sadrozinski, H. F. -W.; Parkinson, P. M. Saz; Thorsett, S. E.; Ziegler, M.] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA. [Bagagli, R.; Bellardi, F.; Bellazzini, R.; Brez, A.; Ceccanti, M.; Corucci, L.; Latronico, L.; Rapposelli, E.; Razzano, M.; Saggini, N.; Sgro, C.; Spandre, G.] Ist Nazl Fis Nucl, Sez Pisa, I-56127 Pisa, Italy. [Ballet, J.; Grenier, I. A.; Landriu, D.; Starck, J. -L.] Univ Paris Diderot, CEA Saclay, CNRS, CEA,IRFU,Lab AIM, F-91191 Gif Sur Yvette, France. [Band, D. L.] NASA, Goddard Space Flight Ctr, CRESST, Greenbelt, MD 20771 USA. [Barbiellini, G.] Ist Nazl Fis Nucl, Sez Trieste, I-34127 Trieste, Italy. [Barbiellini, G.] Univ Trieste, Dipartimento Fis, I-34127 Trieste, Italy. [Baring, M. G.] Rice Univ, Dept Phys & Astron, Houston, TX 77251 USA. [Bastieri, D.; Bisello, D.; Paccagnella, A.; Pieri, L.; Rando, R.; Tibaldo, L.] Ist Nazl Fis Nucl, Sez Padova, I-35131 Padua, Italy. [Bastieri, D.; Bisello, D.; Rando, R.; Tibaldo, L.] Univ Padua, Dipartimento Fis G Galilei, I-35131 Padua, Italy. [Baughman, B. M.; Sander, A.; Smith, P. D.; Winer, B. L.; Ziegler, M.] Ohio State Univ, Dept Phys, Ctr Cosmol & Astroparticle Phys, Columbus, OH 43210 USA. [Bonamente, E.; Ciprini, S.; Germani, S.; Pepe, M.] Ist Nazl Fis Nucl, Sez Perugia, I-06123 Perugia, Italy. [Bonamente, E.; Cecchi, C.; Ciprini, S.; Germani, S.; Lubrano, P.; Pepe, M.] Univ Perugia, Dipartimento Fis, I-06123 Perugia, Italy. [Brigida, M.; Caliandro, G. A.; de Palma, F.; Favuzzi, C.; Fusco, P.; Giglietto, N.; Loparco, F.; Mirizzi, N.; Monte, C.; Raino, S.; Spinelli, P.] Univ Politecn Bari, Dipartimento Fis M Merlin, I-70126 Bari, Italy. [Caliandro, G. A.; de Palma, F.; Favuzzi, C.; Fusco, P.; Giglietto, N.; Loparco, F.; Mirizzi, N.; Monte, C.; Perchiazzi, M.; Raino, S.; Sacchetti, A.; Spinelli, P.] Ist Nazl Fis Nucl, Sez Bari, I-70126 Bari, Italy. [Bruel, P.; Fleury, P.; Giebels, B.; Sanchez, D.] Ecole Polytech, CNRS, IN2P3, Lab Leprince Ringuet, F-91128 Palaiseau, France. [Burnett, T. H.; Roth, M.] Univ Washington, Dept Phys, Seattle, WA 98195 USA. [Camilo, F.; Gotthelf, E. V.] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA. [Caraveo, P. A.; Marelli, M.] INAF Ist Astrofis Spaziale & Fis Cosm, I-20133 Milan, Italy. [Chekhtman, A.; Makeev, A.] George Mason Univ, Fairfax, VA 22030 USA. [Theureau, G.] CNRS, UMR 6115, LPCE, F-45071 Orleans 02, France. [Theureau, G.] Observ Paris, CNRS, INSU, Stn Radioastron Nancay, F-18330 Nancay, France. [Cohen-Tanugi, J.; Farnier, C.; Nuss, E.; Piron, F.] Univ Montpellier 2, CNRS, IN2P3, Lab Phys Theor & Astroparticules, Montpellier, France. [Cominsky, L. R.] Sonoma State Univ, Dept Phys & Astron, Rohnert Pk, CA 94928 USA. [Conrad, J.; Klamra, W.; Pearce, M.; Ryde, F.; Ylinen, T.] Royal Inst Technol, Dept Phys, SE-10691 Stockholm, Sweden. [Conrad, J.; Sellerholm, A.] Stockholm Univ, Dept Phys, SE-10691 Stockholm, Sweden. [Cutini, S.; Gasparrini, D.] ASI, Sci Data Ctr, I-00044 Frascati, Rome, Italy. [Davis, D. S.] Univ Maryland, Ctr Space Sci & Technol, Baltimore, MD 21250 USA. [DeKlotz, M.; Menon, N.] Stellar Solut Inc, Palo Alto, CA 94306 USA. [de Angelis, A.; Giannitrapani, R.] Univ Udine, Dipartimento Fis, I-33100 Udine, Italy. [de Angelis, A.; Giannitrapani, R.] Ist Nazl Fis Nucl, Sez Trieste, Grp Coll Udine, I-33100 Udine, Italy. [Dumora, D.; Guillemot, L.; Lemoine-Goumard, M.; Lott, B.; Parent, D.; Reposeur, T.; Smith, D. A.] CEN Bordeaux Gradignan, CNRS, UMR 5797, IN2P3, F-33175 Gradignan, France. [Dumora, D.; Grondin, M. -H.; Guillemot, L.; Lott, B.] Univ Bordeaux, Ctr Etud Nucl Bordeaux Gradignan, UMR 5797, F-33175 Gradignan, France. [Espinoza, C.; Kramer, M.; Noutsos, A.] Univ Manchester, Jodrell Bank, Ctr Astrophys, Manchester M13 9PL, Lancs, England. [Friere, P. C. C.] Arecibo Observ, Arecibo, PR 00612 USA. [Fukazawa, Y.; Katagiri, H.; Takahashi, H.] Hiroshima Univ, Dept Phys Sci, Higashihiroshima 7398526, Japan. [Fukazawa, Y.; Katagiri, H.; Takahashi, H.] Hiroshima Univ, Hiroshima Astrophys Sci Ctr, Higashihiroshima 7398526, Japan. [Gehrels, N.; Ritz, S.] Univ Maryland, College Pk, MD 20742 USA. [Hobbs, G.; Johnston, S.; Manchester, R. N.] CSIRO, Australia Telescope Natl Facil, Epping, NSW 1710, Australia. [Kanbach, G.; Orlando, E.; Strong, A. W.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Kaspi, V. M.; Livingstone, M.] McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada. [Kataoka, J.; Kawai, N.; Nakamori, T.] Tokyo Inst Technol, Dept Phys, Meguro, Tokyo 1528551, Japan. [Kawai, N.] RIKEN, Cosm Radiat Lab, Wako, Saitama 3510198, Japan. [Kiziltan, B.] UCO Lick Observ, Santa Cruz, CA 95064 USA. [Knodlseder, J.; Vilchez, N.] CNRS, UPS, Ctr Etud Spatiale Rayonnements, F-31028 Toulouse 4, France. [Lee, B.] Orbital Network Engn, Cupertino, CA 95014 USA. [McLaughlin, M. A.] W Virginia Univ, Dept Phys, Morgantown, WV 26506 USA. [Mineo, T.] IASF Palermo, I-90146 Palermo, Italy. [Moretti, E.; Vitale, V.] Ist Nazl Fis Nucl, Sez Roma Tor Vergata, I-00133 Rome, Italy. [Morselli, A.; Vitale, V.] Univ Roma Tor Vergata, Dipartimento Fis, I-00133 Rome, Italy. [Ormes, J. F.] Univ Denver, Dept Phys & Astron, Denver, CO 80208 USA. [Ozaki, M.; Takahashi, T.] Japan Aerosp Explorat Agcy, Inst Space & Astronaut Sci, JAXA, Sagamihara, Kanagawa 2298510, Japan. [Paccagnella, A.] Univ Padua, Dipartimento Ingn Informaz, I-35131 Padua, Italy. [Ransom, S. M.] Natl Radio Astron Observ, Charlottesville, VA 22903 USA. [Reyes, L. C.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA. [Rodriguez, A. Y.; Torres, D. F.] CSIC, Inst Ciencies Espai, IEEC, Barcelona 08193, Spain. [Siskind, E. J.] NYCB Real Time Comp Inc, Lattingtown, NY 11560 USA. [Suson, D. J.] Purdue Univ Calumet, Dept Chem & Phys, Hammond, IN 46323 USA. [Tibolla, O.] Heidelberg Univ, D-69117 Heidelberg, Germany. [Torres, D. F.] ICREA, Barcelona, Spain. [Tramacere, A.] CIFS, I-10133 Turin, Italy. [Ylinen, T.] Univ Kalmar, Sch Pure & Appl Nat Sci, SE-39182 Kalmar, Sweden. RP Abdo, AA (reprint author), USN, Res Lab, Div Space Sci, Washington, DC 20375 USA. EM massimiliano.razzano@pi.infn.it; rwr@astro.stanford.edu RI Hays, Elizabeth/D-3257-2012; Johnson, Neil/G-3309-2014; Reimer, Olaf/A-3117-2013; Funk, Stefan/B-7629-2015; Loparco, Francesco/O-8847-2015; Johannesson, Gudlaugur/O-8741-2015; Gargano, Fabio/O-8934-2015; Moskalenko, Igor/A-1301-2007; Mazziotta, Mario /O-8867-2015; Sgro, Carmelo/K-3395-2016; Torres, Diego/O-9422-2016; Orlando, E/R-5594-2016; Starck, Jean-Luc/D-9467-2011; Thompson, David/D-2939-2012; Stecker, Floyd/D-3169-2012; Harding, Alice/D-3160-2012; Gehrels, Neil/D-2971-2012; McEnery, Julie/D-6612-2012; Baldini, Luca/E-5396-2012; lubrano, pasquale/F-7269-2012; Morselli, Aldo/G-6769-2011; Nolan, Patrick/A-5582-2009; Kuss, Michael/H-8959-2012; giglietto, nicola/I-8951-2012; Ozaki, Masanobu/K-1165-2013; Rando, Riccardo/M-7179-2013 OI Moretti, Elena/0000-0001-5477-9097; Cutini, Sara/0000-0002-1271-2924; Berenji, Bijan/0000-0002-4551-772X; Gasparrini, Dario/0000-0002-5064-9495; Tramacere, Andrea/0000-0002-8186-3793; Baldini, Luca/0000-0002-9785-7726; Marelli, Martino/0000-0002-8017-0338; Giordano, Francesco/0000-0002-8651-2394; Thorsett, Stephen/0000-0002-2025-9613; Mineo, Teresa/0000-0002-4931-8445; Stephens, Thomas/0000-0003-3065-6871; De Angelis, Alessandro/0000-0002-3288-2517; Frailis, Marco/0000-0002-7400-2135; Caraveo, Patrizia/0000-0003-2478-8018; Bastieri, Denis/0000-0002-6954-8862; Omodei, Nicola/0000-0002-5448-7577; Pesce-Rollins, Melissa/0000-0003-1790-8018; Ransom, Scott/0000-0001-5799-9714; Reimer, Olaf/0000-0001-6953-1385; Funk, Stefan/0000-0002-2012-0080; Loparco, Francesco/0000-0002-1173-5673; Johannesson, Gudlaugur/0000-0003-1458-7036; Gargano, Fabio/0000-0002-5055-6395; Moskalenko, Igor/0000-0001-6141-458X; Mazziotta, Mario /0000-0001-9325-4672; Torres, Diego/0000-0002-1522-9065; Rando, Riccardo/0000-0001-6992-818X; Sgro', Carmelo/0000-0001-5676-6214; Starck, Jean-Luc/0000-0003-2177-7794; Thompson, David/0000-0001-5217-9135; lubrano, pasquale/0000-0003-0221-4806; Morselli, Aldo/0000-0002-7704-9553; giglietto, nicola/0000-0002-9021-2888; FU National Aeronautics and Space Administration; Department of Energy in the United States; Commissariat a l'Energie Atomique; Centre National de la Recherche Scientifique/Institut National de Physique Nucleaire et de Physique des Particules in France; Agenzia Spaziale Italiana; Istituto Nazionale di Fisica Nucleare; Istituto Nazionale di Astrofisica in Italy; Ministry of Education, Culture, Sports, Science and Technology (MEXT); High Energy Accelerator Research Organization (KEK); Japan Aerospace Exploration Agency (JAXA); K. A. Wallenberg Foundation; Swedish National Space Board; Commonwealth of Australia FX The Fermi LAT Collaboration acknowledges the generous support of a number of agencies and institutes that have supported the development of the LAT. These include the National Aeronautics and Space Administration and the Department of Energy in the United States, the Commissariat a l'Energie Atomique and the Centre National de la Recherche Scientifique/Institut National de Physique Nucleaire et de Physique des Particules in France, the Agenzia Spaziale Italiana, the Istituto Nazionale di Fisica Nucleare, and the Istituto Nazionale di Astrofisica in Italy, the Ministry of Education, Culture, Sports, Science and Technology (MEXT), High Energy Accelerator Research Organization (KEK) and Japan Aerospace Exploration Agency (JAXA) in Japan, and the K. A. Wallenberg Foundation and the Swedish National Space Board in Sweden. The Australia Telescope is funded by the Commonwealth of Australia for operation as a National Facility managed by the CSIRO. NR 41 TC 102 Z9 102 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD MAY 10 PY 2009 VL 696 IS 2 BP 1084 EP 1093 DI 10.1088/0004-637X/696/2/1084 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 441IO UT WOS:000265762700003 ER PT J AU Mousis, O Marboeuf, U Lunine, JI Alibert, Y Fletcher, LN Orton, GS Pauzat, F Ellinger, Y AF Mousis, Olivier Marboeuf, Ulysse Lunine, Jonathan I. Alibert, Yann Fletcher, Leigh N. Orton, Glenn S. Pauzat, Francoise Ellinger, Yves TI DETERMINATION OF THE MINIMUM MASSES OF HEAVY ELEMENTS IN THE ENVELOPES OF JUPITER AND SATURN SO ASTROPHYSICAL JOURNAL LA English DT Article DE planetary systems; planetary systems: formation; solar system: formation ID OUTER SOLAR-SYSTEM; GIANT PLANETS; PROTOPLANETARY DISKS; INTERSTELLAR ICES; JOVIAN SUBNEBULA; ABUNDANCE; CARBON; PROBE; ATMOSPHERE; VOLATILES AB We calculate the minimum mass of heavy elements required in the envelopes of Jupiter and Saturn to match the observed oversolar abundances of volatiles. Because the clathration efficiency remains unknown in the solar nebula, we have considered a set of sequences of ice formation in which the fraction of water available for clathration is varied between 0 and 100%. In all the cases considered, we assume that the water abundance remains homogeneous whatever the heliocentric distance in the nebula and directly derives from a gas phase of solar composition. Planetesimals then form in the feeding zones of Jupiter and Saturn from the agglomeration of clathrates and pure condensates in proportions fixed by the clathration efficiency. A fraction of Kr and Xe may have been sequestrated by the H(3)(+) ion in the form of stable XeH(3)(+) and KrH(3)(+) complexes in the solar nebula gas phase, thus implying the formation of at least partly Xe- and Kr-impoverished planetesimals in the feeding zones of Jupiter and Saturn. These planetesimals were subsequently accreted and vaporized into the hydrogen envelopes of Jupiter and Saturn, thus engendering volatiles enrichments in their atmospheres, with respect to hydrogen. Taking into account both refractory and volatile components, and assuming plausible molecular mixing ratios in the gas phase of the outer solar nebula, we show that it is possible to match the observed enrichments in Jupiter and Saturn, whatever the clathration efficiency. Our calculations predict that the O/H enrichment decreases from similar to 5.5 to 5.1 time (O/H)(circle dot) in the envelope of Jupiter and from 15.2 to 14.1 times(O/H)(circle dot) in the envelope of Saturn with the growing clathration efficiency in the solar nebula. As a result, the minimum mass of ices needed to be injected in the envelope of Jupiter decreases from similar to 20.0 to 18.6 M(circle plus), including a mass of water diminishing from 10.4 to 9.3 M(circle plus). In the same conditions, the minimum mass of ices needed in the envelope of Saturn decreases from similar to 16.7 to 15.6 M(circle plus), including amass of water diminishing from 8.6 to 7.7 M(circle plus). The accretion of planetesimals with ices to rocks ratios similar to 1 in the envelope of Jupiter, namely a value derived from the bulk densities of Ganymede and Callisto, remains compatible with the mass of heavy elements predicted by interior models. On the other hand, the accretion of planetesimals with similar ice-to-rock in the envelope of Saturn implies a mass of heavy elements greater than the one predicted by interior models, unless a substantial fraction of the accreted rock and water sedimented onto the core of the planet during its evolution. C1 [Mousis, Olivier; Lunine, Jonathan I.] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA. [Mousis, Olivier; Marboeuf, Ulysse; Alibert, Yann] Observ Besancon, CNRS, UMR 6213, Inst UTINAM, F-25010 Besancon, France. [Fletcher, Leigh N.; Orton, Glenn S.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Pauzat, Francoise; Ellinger, Yves] Univ Paris 06, Chim Theor Lab, CNRS, LETMEX,UMR 7616, F-75252 Paris 05, France. RP Mousis, O (reprint author), Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA. EM mousis@lpl.arizona.edu RI Fletcher, Leigh/D-6093-2011 OI Fletcher, Leigh/0000-0001-5834-9588 FU ANR HOLMES; French Centre National d'Etudes Spatiales; Juno Project; NASA FX O.M. and U.M. acknowledge the financial support of the ANR HOLMES. This work was supported in part by the French Centre National d'Etudes Spatiales. J.I.L. was supported by the Juno Project at the Southwest Research Institute. L.N.F. was supported by an appointment to the NASA Postdoctoral Program at the Jet Propulsion Laboratory, administered by Oak Ridge Associated Universities through a contract with NASA. Tristan Guillot is acknowledged for helpful discussions. NR 45 TC 39 Z9 39 U1 0 U2 7 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAY 10 PY 2009 VL 696 IS 2 BP 1348 EP 1354 DI 10.1088/0004-637X/696/2/1348 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 441IO UT WOS:000265762700021 ER PT J AU Zenitani, S Hesse, M Klimas, A AF Zenitani, Seiji Hesse, Michael Klimas, Alex TI TWO-FLUID MAGNETOHYDRODYNAMIC SIMULATIONS OF RELATIVISTIC MAGNETIC RECONNECTION SO ASTROPHYSICAL JOURNAL LA English DT Article DE magnetic fields; MHD; plasmas; relativity ID STRIPED PULSAR WIND; PARTICLE-ACCELERATION; NEUTRON-STARS; CURRENT SHEET; PAIR PLASMAS; RADIATIVE MECHANISM; NUMERICAL SCHEME; GALACTIC NUCLEI; GRB OUTFLOWS; DISSIPATION AB We investigate the large-scale evolution of a relativistic magnetic reconnection in an electron-positron pair plasma by a relativistic two-fluid magnetohydrodynamic (MHD) code. We introduce an interspecies friction force as an effective resistivity to dissipate magnetic fields. We demonstrate that magnetic reconnection successfully occurs in our two-fluid system, and that it involves Petschek-type bifurcated current layers in a later stage. We further observe a quasi-steady evolution thanks to an open boundary condition, and find that the Petschek-type structure is stable over the long time period. Simulation results and theoretical analyses exhibit that the Petschek outflow channel becomes narrower when the reconnection inflow contains more magnetic energy, as previously claimed. Meanwhile, we find that the reconnection rate goes up to similar to 1 in extreme cases, which is faster than previously thought. The role of the resistivity, implications for reconnection models in the magnetically dominated limit, and relevance to kinetic reconnection works are discussed. C1 [Zenitani, Seiji; Hesse, Michael; Klimas, Alex] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Zenitani, S (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. EM Seiji.Zenitani-1@nasa.gov RI Hesse, Michael/D-2031-2012; Zenitani, Seiji/D-7988-2013; NASA MMS, Science Team/J-5393-2013 OI Zenitani, Seiji/0000-0002-0945-1815; NASA MMS, Science Team/0000-0002-9504-5214 FU NASA Center for Computational Sciences; NASA's MMS SMART mission FX The authors are grateful to N. Watanabe, R. Yoshitake, and M. Kuznetsova for helpful comments. The authors thank the anonymous referee for his/her constructive comments which helped them to improve the manuscript. This research was supported by the NASA Center for Computational Sciences, and NASA's MMS SMART mission. S.Z. gratefully acknowledges support from NASA's postdoctoral program. NR 65 TC 49 Z9 49 U1 1 U2 6 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD MAY 10 PY 2009 VL 696 IS 2 BP 1385 EP 1401 DI 10.1088/0004-637X/696/2/1385 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 441IO UT WOS:000265762700025 ER PT J AU Wang, TJ Ofman, L Davila, JM AF Wang, T. J. Ofman, L. Davila, J. M. TI PROPAGATING SLOW MAGNETOACOUSTIC WAVES IN CORONAL LOOPS OBSERVED BY HINODE/EIS SO ASTROPHYSICAL JOURNAL LA English DT Article DE Sun: corona; Sun: flares; Sun: oscillations; Sun: UV radiation; Sun: X-rays, gamma rays ID TRANSITION REGION OSCILLATIONS; EUV IMAGING SPECTROMETER; LONGITUDINAL INTENSITY OSCILLATIONS; MAGNETIC-FIELD; PHOTOSPHERIC OSCILLATIONS; MAGNETOSONIC WAVES; SOLAR CHROMOSPHERE; OBSERVED HEIGHTS; ACOUSTIC-WAVES; MHD WAVES AB We present the first Hinode/EUV Imaging Spectrometer observations of 5 minute quasi-periodic oscillations detected in a transition-region line (He II) and five coronal lines (Fe X, Fe XII, Fe XIII, Fe XIV, and Fe XV) at the footpoint of a coronal loop. The oscillations exist throughout the whole observation, characterized by a series of wave packets with nearly constant period, typically persisting for 4-6 cycles with a lifetime of 20-30 minutes. There is an approximate in-phase relation between Doppler shift and intensity oscillations. This provides evidence for slow magnetoacoustic waves propagating upward from the transition region into the corona. We find that the oscillations detected in the five coronal lines are highly correlated, and the amplitude decreases with increasing temperature. The amplitude of Doppler shift oscillations decrease by a factor of about 3, while that of relative intensity decreases by a factor of about 4 from Fe X to Fe XV. These oscillations may be caused by the leakage of the photospheric p-modes through the chromosphere and transition region into the corona, which has been suggested as the source for intensity oscillations previously observed by Transition Region and Coronal Explorer. The temperature dependence of the oscillation amplitudes can be explained by damping of the waves traveling along the loop with multithread structure near the footpoint. Thus, this property may have potential value for coronal seismology in diagnostic of temperature structure in a coronal loop. C1 [Wang, T. J.; Ofman, L.] Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA. [Wang, T. J.; Ofman, L.; Davila, J. M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Wang, TJ (reprint author), Catholic Univ Amer, Dept Phys, 620 Michigan Ave, Washington, DC 20064 USA. EM wangtj@helio.gsfc.nasa.gov FU ESA; NSC; NRL [N00173-06-1-G033]; NASA [NNG06GI55G] FX Hinode is a Japanese mission developed, launched, and operated by ISAS/JAXA in partnership with NAOJ, NASA, and STFC (UK). Additional operation support is provided by ESA and NSC (Norway). T.J.W. is grateful to Drs. Ignacio Ugarte-Utta and David Williams for their valuable discussions and suggestions. The authors also thank Dr. Harry Warren and the EIS team in NRL for providing EIS data analysis tutorials. The work of L.O. and T.J.W. was supported by NRL grant N00173-06-1-G033. L.O. was also supported by NASA grant NNG06GI55G. NR 59 TC 59 Z9 59 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAY 10 PY 2009 VL 696 IS 2 BP 1448 EP 1460 DI 10.1088/0004-637X/696/2/1448 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 441IO UT WOS:000265762700031 ER PT J AU Yamaguchi, H Katsuda, S AF Yamaguchi, H. Katsuda, S. TI SUZAKU SPECTROSCOPY OF VELA SHRAPNEL B SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM: individual (Vela SNR); supernova remnants; X-rays: ISM ID X-RAY SPECTROSCOPY; SUPERNOVA REMNANT; CASSIOPEIA-A; PUPPIS-A; EJECTA; DISCOVERY; ABUNDANCES; EMISSION; MODELS; KNOTS AB We present the X-ray observation of Vela shrapnel B with the X-ray Imaging Spectrometer on board the Suzaku satellite. The shrapnel is one of several ejecta fragmentlike features protruding beyond the primary blast wave shock front of the Vela supernova remnant. The spectrum of shrapnel B is well represented by a single-temperature thin-thermal plasma in a nonequilibrium ionization state. The elemental abundances of O, Ne, and Mg are found to be significantly higher than the solar values, supporting that shrapnel B originates from supernova ejecta. The abundances of O, Ne, and Mg relative to Fe are enhanced above their solar values, while that of Si relative to Fe are at their solar values. This abundance pattern is similar to that in shrapnel D, except that the enhancements of the lighter elements are less prominent, suggesting more extensive mixing with the interstellar medium (ISM) in shrapnel B. The contribution of the ISM is considered to be larger at the trailing region, because the absolute abundances of some elements there are depleted relative to those at the shrapnel's head. C1 [Yamaguchi, H.] RIKEN, Inst Phys & Chem Res, Wako, Saitama 3510198, Japan. [Katsuda, S.] Osaka Univ, Dept Earth & Space Sci, Osaka 5600043, Japan. [Katsuda, S.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Yamaguchi, H (reprint author), RIKEN, Inst Phys & Chem Res, 2-1 Hirosawa, Wako, Saitama 3510198, Japan. EM hiroya@crab.riken.jp RI XRAY, SUZAKU/A-1808-2009 FU Special Postdoctoral Researchers Program in RIKEN; Japan Society for Promotion of Science (JSPS) FX The authors deeply appreciate the helpful comments on revising the manuscript from Una Hwang. A number of constructive suggestions from the referee greatly helped us to improve the quality of the paper. We also thank Junko S. Hiraga for useful discussions. H. Y. is supported by the Special Postdoctoral Researchers Program in RIKEN. S. K. is a Research Fellow of Japan Society for Promotion of Science (JSPS). NR 27 TC 4 Z9 4 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 MAY 10 PY 2009 VL 696 IS 2 BP 1548 EP 1553 DI 10.1088/0004-637X/696/2/1548 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 441IO UT WOS:000265762700042 ER PT J AU Lee, CF Hsu, MC Sahai, R AF Lee, Chin-Fei Hsu, Ming-Chien Sahai, Raghvendra TI COLLIMATED FAST WIND IN THE PREPLANETARY NEBULA CRL 618 SO ASTROPHYSICAL JOURNAL LA English DT Article DE planetary nebulae: general; stars: AGB and post-AGB; stars: mass loss; stars: winds, outflows ID PLANETARY-NEBULAE; PROTOPLANETARY NEBULAE; MOLECULE FORMATION; INFRARED-EMISSION; BIPOLAR NEBULAE; MASS-LOSS; JETS; OUTFLOWS; MULTIPLE; STELLAR AB Collimated fast winds (CFWs) have been proposed to operate during the post asymptotic giant branch (post-AGB) evolutionary phase (and even earlier during the late AGB phase), responsible for the shaping of preplanetary nebulae (PPNs) and young planetary nebulae (PNs). This paper is a follow-up to our previous study of CFW models for the well-studied PPN CRL 618. Previously, we compared our CFW models with optical observations of CRL 618 in atomic and ionic lines and found that a CFW with a small opening angle can readily reproduce the highly collimated shape of the northwestern (W1) lobe of CRL 618 and the bowlike structure seen at its tip. In this paper, we compare our CFW models with recent observations of CRL 618 in CO J = 2-1, J = 65, and H(2) 1-0 S(1). In our models, limb-brightened shell structures are seen in CO and H(2) at low velocity (LV) arising from the shocked AGB wind in the shell, and can be identified as the LV components in the observations. However, the shell structure in CO J = 2-1 is significantly less extended than that seen in the observations. None of our models can properly reproduce the observed high-velocity (HV) molecular emission near the source along the body of the lobe. In order to reproduce the HV molecular emission in CRL 618, the CFW is required to have a different structure. One possible CFW structure is the cylindrical jet, with the fast wind material confined to a small cross section and collimated to the same direction along the outflow axis. C1 [Lee, Chin-Fei; Hsu, Ming-Chien] Acad Sinica, Inst Astron & Astrophys, Taipei 106, Taiwan. [Sahai, Raghvendra] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Lee, CF (reprint author), Acad Sinica, Inst Astron & Astrophys, POB 23-141, Taipei 106, Taiwan. EM cflee@asiaa.sinica.edu.tw FU NSC [NSC96-2112-M-001-014-MY3]; NASA [NMO710840-102898, NAS5-26555]; Space Telescope Science Institute [GO-10317.01]; National Aeronautics and Space Administration FX C.-F.L. and M.-C.H. are financially supported in part by the NSC grant NSC96-2112-M-001-014-MY3. R.S. thanks NASA for funding this work via an LTSA award (NMO710840-102898); R.S. also received partial support for this work from an HST GO award (no. GO-10317.01) from the Space Telescope Science Institute (operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS5-26555). Some of the research described in this paper was carried out by R.S. at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. NR 35 TC 21 Z9 21 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAY 10 PY 2009 VL 696 IS 2 BP 1630 EP 1639 DI 10.1088/0004-637X/696/2/1630 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 441IO UT WOS:000265762700049 ER PT J AU Eguchi, S Ueda, Y Terashima, Y Mushotzky, R Tueller, J AF Eguchi, Satoshi Ueda, Yoshihiro Terashima, Yuichi Mushotzky, Richard Tueller, Jack TI SUZAKU VIEW OF THE SWIFT/BAT ACTIVE GALACTIC NUCLEI. I. SPECTRAL ANALYSIS OF SIX ACTIVE GALACTIC NUCLEI AND EVIDENCE FOR TWO TYPES OF OBSCURED POPULATION SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: active; gamma rays: observations; X-rays: galaxies; X-rays: general ID SUPERMASSIVE BLACK-HOLES; X-RAY-SPECTRUM; SEYFERT-GALAXIES; XMM-NEWTON; BAT SURVEY; ABSORPTION; CHANDRA; STARBURSTS; ABUNDANCES; EVOLUTION AB We present a systematic spectral analysis with Suzaku of six active galactic nuclei (AGNs) detected in the Swift/BAT hard X-ray (15-200 keV) survey: Swift J0138.6-4001, J0255.2-0011, J0350.1-5019, J0505.7-2348, J0601.9-8636, and J1628.1-5145. This is considered to be a representative sample of new AGNs without X-ray spectral information before the BAT survey. We find that the 0.5-200 keV spectra of these sources can be uniformly fitted with a base model consisting of heavily absorbed (log N-H > 23.5 cm(-2)) transmitted components, scattered lights, a reflection component, and an iron-K emission line. There are two distinct groups: three "new-type" AGNs (including the two sources reported by Ueda et al.) with an extremely small scattered fraction (f(scat) < 0.5%) and strong reflection component (R = Omega/2 pi greater than or similar to 0.8, where Omega is the solid angle of the reflector), and three "classical-type" ones with f(scat) > 0.5% and R less than or similar to 0.8. The spectral parameters suggest that the new type has an optically thick torus for Thomson scattering (N-H similar to 10(25) cm(-2)) with a small opening angle theta similar to 20 degrees. viewed in a rather face-on geometry, while the classical type has a thin torus (N-H similar to 10(23-24) cm(-2)) with theta greater than or similar to 30 degrees. We infer that a significant number of new-type AGNs with an edge-on view are missing in the current all-sky hard X-ray surveys. C1 [Eguchi, Satoshi; Ueda, Yoshihiro] Kyoto Univ, Dept Astron, Kyoto 6068502, Japan. [Terashima, Yuichi] Ehime Univ, Dept Phys, Fac Sci, Matsuyama, Ehime 7908577, Japan. [Mushotzky, Richard; Tueller, Jack] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Eguchi, S (reprint author), Kyoto Univ, Dept Astron, Kyoto 6068502, Japan. RI Tueller, Jack/D-5334-2012; XRAY, SUZAKU/A-1808-2009 FU JSPS [20540230, 20740109]; Ministry of Education, Culture, Sports, Science and Technology (MEXT) of Japan; National Aeronautics and Space Administration FX We thank Lisa Winter for useful comments to the manuscript. Part of this work was financially supported by Grants-in-Aid for JSPS Fellows ( S. E.), for Scientific Research 20540230 and 20740109, and for the Global COE Program "The Next Generation of Physics, Spun from Universality and Emergence" from the Ministry of Education, Culture, Sports, Science and Technology (MEXT) of Japan. This research has made use of the NASA/IPAC Extragalactic Database (NED) which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. NR 35 TC 29 Z9 29 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 MAY 10 PY 2009 VL 696 IS 2 BP 1657 EP 1667 DI 10.1088/0004-637X/696/2/1657 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 441IO UT WOS:000265762700051 ER PT J AU Wyder, TK Martin, DC Barlow, TA Foster, K Friedman, PG Morrissey, P Neff, SG Neill, JD Schiminovich, D Seibert, M Bianchi, L Donas, J Heckman, TM Lee, YW Madore, BF Milliard, B Rich, RM Szalay, AS Yi, SK AF Wyder, Ted K. Martin, D. Christopher Barlow, Tom A. Foster, Karl Friedman, Peter G. Morrissey, Patrick Neff, Susan G. Neill, James D. Schiminovich, David Seibert, Mark Bianchi, Luciana Donas, Jose Heckman, Timothy M. Lee, Young-Wook Madore, Barry F. Milliard, Bruno Rich, R. Michael Szalay, Alex S. Yi, Sukyoung K. TI THE STAR FORMATION LAW AT LOW SURFACE DENSITY SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: evolution; galaxies: irregular; galaxies: ISM; galaxies: spiral; ultraviolet: galaxies ID BRIGHTNESS DISK GALAXIES; EXTREME OUTER DISK; INTERSTELLAR-MEDIUM; MOLECULAR GAS; FORMATION THRESHOLDS; FORMING GALAXIES; NEARBY GALAXIES; LUMINOSITY FUNCTION; INFRARED PROPERTIES; STARBURST GALAXIES AB We investigate the nature of the star formation law at low gas surface densities using a sample of 19 low surface brightness (LSB) galaxies with existing H I maps in the literature, UV imaging from the Galaxy Evolution Explorer satellite, and optical images from the Sloan Digital Sky Survey. All of the LSB galaxies have (NUV - r) colors similar to those for higher surface brightness star-forming galaxies of similar luminosity indicating that their average star formation histories are not very different. Based upon four LSB galaxies with both UV and far-infrared (FIR) data, we find FIR/UV ratios significantly less than 1, implying low amounts of internal UV extinction in LSB galaxies. We use the UV images and H I maps to measure the star formation rate (SFR) and hydrogen gas surface density within the same region for all the galaxies. The LSB galaxy star formation rate surface densities lie below the extrapolation of the power law fit to the SFR surface density as a function of the total gas density for higher surface brightness galaxies. Although there is more scatter, the LSB galaxies also lie below a second version of the star formation law in which the SFR surface density is correlated with the gas density divided by the orbital time in the disk. The downturn seen in both star formation laws is consistent with theoretical models that predict lower star formation efficiencies in LSB galaxies due to the declining molecular fraction with decreasing density. C1 [Wyder, Ted K.; Martin, D. Christopher; Barlow, Tom A.; Foster, Karl; Friedman, Peter G.; Morrissey, Patrick; Neill, James D.] CALTECH, Pasadena, CA 91125 USA. [Neff, Susan G.] NASA, Goddard Space Flight Ctr, Astron & Solar Phys Lab, Greenbelt, MD 20771 USA. [Schiminovich, David] Columbia Univ, Dept Astron, New York, NY 10027 USA. [Seibert, Mark; Madore, Barry F.] Observ Carnegie Inst Washington, Pasadena, CA 91101 USA. [Bianchi, Luciana] Johns Hopkins Univ, Ctr Astrophys Sci, Baltimore, MD 21218 USA. [Donas, Jose; Milliard, Bruno] Astrophys Lab, F-13376 Marseille 12, France. [Heckman, Timothy M.; Szalay, Alex S.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Lee, Young-Wook; Yi, Sukyoung K.] Yonsei Univ, Ctr Space Astrophys, Seoul 120749, South Korea. [Rich, R. Michael] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA. RP Wyder, TK (reprint author), CALTECH, MC 278-17,1200 E Calif Blvd, Pasadena, CA 91125 USA. NR 76 TC 63 Z9 63 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAY 10 PY 2009 VL 696 IS 2 BP 1834 EP 1853 DI 10.1088/0004-637X/696/2/1834 PG 20 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 441IO UT WOS:000265762700066 ER PT J AU Gaidos, E Krot, AN Williams, JP Raymond, SN AF Gaidos, Eric Krot, Alexander N. Williams, Jonathan P. Raymond, Sean N. TI Al-26 AND THE FORMATION OF THE SOLAR SYSTEM FROM A MOLECULAR CLOUD CONTAMINATED BY WOLF-RAYET WINDS SO ASTROPHYSICAL JOURNAL LA English DT Review DE planetary systems: formation; planetary systems: protoplanetary disks ID ALUMINUM-RICH INCLUSIONS; SHORT-LIVED RADIONUCLIDES; ORION-NEBULA-CLUSTER; OXYGEN ISOTOPIC COMPOSITIONS; M-CIRCLE-DOT; REFRACTORY INCLUSIONS; STAR-FORMATION; MASSIVE STARS; CARBONACEOUS CHONDRITE; PROTOPLANETARY DISKS AB In agreement with previous work, we show that the presence of the short-lived radionuclide (SLR) Al-26 in the early solar system was unlikely (less than 2% a priori probability) to be the result of direct introduction of supernova (SN) ejecta into the gaseous disk during the Class II stage of protosolar evolution. We also show that Bondi-Hoyle accretion of any contaminated residual gas from the Sun's natal star cluster contributed negligible Al-26 to the primordial solar system. Our calculations are consistent with the absence of the oxygen isotopic signature expected with any late introduction of SN ejecta into the protoplanetary disk. Instead, the presence of Al-26 in the oldest solar system solids (calcium-aluminum-rich inclusions (CAIs)) and its apparent uniform distribution with the inferred canonical Al-26/Al-27 ratio of (4.5-5) x 10(-5) support the inheritance of Al-26 from the Sun's parent giant molecular cloud. We propose that this radionuclide originated in a prior generation of massive stars that formed in the same molecular cloud and contaminated that cloud by Wolf-Rayet winds. We calculated the Galactic distribution of Al-26/Al-27 ratios that arise from such contamination using the established embedded cluster mass and stellar initial mass functions, published nucleosynthetic yields from the winds of massive stars, and by assuming rapid and uniform mixing into the cloud. Although our model predicts that the majority of stellar systems contain no Al-26 from massive stars, and that the a priori probability that the Al-26/Al-27 ratio will reach or exceed the canonical solar system value is only similar to 6%, the maximum in the distribution of nonzero values is close to the canonical Al-26/Al-27 ratio. We find that the Sun most likely formed 4-5 million years (Myr) after the massive stars that were the source of Al-26. Furthermore, our model can explain the initial solar system abundance of a second, co-occurring SLR, Ca-41, if similar to 5 x 10(5) yr elapsed between ejection of the radionuclides and the formation of CAIs. The presence of a third radionuclide, Fe-60, can be quantitatively explained if (1) the Sun formed immediately after the first SNe from the earlier generation of stars; (2) only 5% of SN ejecta was incorporated into the molecular cloud, or (3) the radionuclide originated in an even earlier generation of stars whose contributions to other radionuclides with a shorter half-life had completely decayed. C1 [Gaidos, Eric] Univ Hawaii, Dept Geol & Geophys, Honolulu, HI 96822 USA. [Krot, Alexander N.] Univ Hawaii, Hawaii Inst Geophys & Planetol, Honolulu, HI 96822 USA. [Williams, Jonathan P.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. RP Gaidos, E (reprint author), NASA Astrobiol Inst, Washington, DC USA. EM gaidos@hawaii.edu; sasha@higp.hawaii.edu; jpw@ifa.hawaii.edu; sean.raymond@colorado.edu OI Williams, Jonathan/0000-0001-5058-695X FU NASA Astrobiology Institute [NNA04CC08A] FX This material is based upon work supported by the National Aeronautics and Space Administration through the NASA Astrobiology Institute under Cooperative Agreement No. NNA04CC08A issued through the Office of Space Science. S. R. is a NASA Postdoctoral Program Fellow. Some of this work was performed while E. G. was a Visiting Scholar at the University of California Berkeley. We thank Gary Huss and Kazuhide Nagashima for enlightening discussions and John Bally and Marcel Arnould for helpful comments and corrections. NR 135 TC 44 Z9 44 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAY 10 PY 2009 VL 696 IS 2 BP 1854 EP 1863 DI 10.1088/0004-637X/696/2/1854 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 441IO UT WOS:000265762700067 ER PT J AU Perley, DA Metzger, BD Granot, J Butler, NR Sakamoto, T Ramirez-Ruiz, E Levan, AJ Bloom, JS Miller, AA Bunker, A Chen, HW Filippenko, AV Gehrels, N Glazebrook, K Hall, PB Hurley, KC Kocevski, D Li, W Lopez, S Norris, J Piro, AL Poznanski, D Prochaska, JX Quataert, E Tanvir, N AF Perley, D. A. Metzger, B. D. Granot, J. Butler, N. R. Sakamoto, T. Ramirez-Ruiz, E. Levan, A. J. Bloom, J. S. Miller, A. A. Bunker, A. Chen, H-W. Filippenko, A. V. Gehrels, N. Glazebrook, K. Hall, P. B. Hurley, K. C. Kocevski, D. Li, W. Lopez, S. Norris, J. Piro, A. L. Poznanski, D. Prochaska, J. X. Quataert, E. Tanvir, N. TI GRB 080503: IMPLICATIONS OF A NAKED SHORT GAMMA-RAY BURST DOMINATED BY EXTENDED EMISSION SO ASTROPHYSICAL JOURNAL LA English DT Review DE gamma rays: bursts ID NEUTRON-STAR MERGERS; AFTERGLOW LIGHT CURVES; COMPACT BINARY MERGER; HOST GALAXY; BLACK-HOLE; BATSE OBSERVATIONS; OPTICAL AFTERGLOW; DURATION GRB; LONG; PROGENITORS AB We report on observations of GRB 080503, a short gamma-ray burst (GRB) with very bright extended emission (about 30 times the gamma-ray fluence of the initial spike) in conjunction with a thorough comparison to other short Swift events. In spite of the prompt-emission brightness, however, the optical counterpart is extraordinarily faint, never exceeding 25 mag in deep observations starting at similar to 1 hr after the Burst Alert Telescope (BAT) trigger. The optical brightness peaks at similar to 1 day and then falls sharply in a manner similar to the predictions of Li & Paczynski (1998) for supernova-like emission following compact binary mergers. However, a shallow spectral index and similar evolution in X-rays inferred from Chandra observations are more consistent with an afterglow interpretation. The extreme faintness of this probable afterglow relative to the bright gamma-ray emission argues for a very low density medium surrounding the burst (a "naked" GRB), consistent with the lack of a coincident host galaxy down to 28.5 mag in deep Hubble Space Telescope imaging. The late optical and X-ray peak could be explained by a slightly off-axis jet or by a refreshed shock. Our observations reinforce the notion that short GRBs generally occur outside regions of active star formation, but demonstrate that in some cases the luminosity of the extended prompt emission can greatly exceed that of the short spike, which may constrain theoretical interpretation of this class of events. This extended emission is not the onset of an afterglow, and its relative brightness is probably either a viewing-angle effect or intrinsic to the central engine itself. Because most previous BAT short bursts without observed extended emission are too faint for this signature to have been detectable even if it were present at typical level, conclusions based solely on the observed presence or absence of extended emission in the existing Swift sample are premature. C1 [Perley, D. A.; Metzger, B. D.; Butler, N. R.; Bloom, J. S.; Miller, A. A.; Filippenko, A. V.; Li, W.; Piro, A. L.; Poznanski, D.; Quataert, E.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Granot, J.] Univ Hertfordshire, Ctr Astrophys Res, Hatfield AL10 9AB, Herts, England. [Sakamoto, T.; Gehrels, N.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Sakamoto, T.] Univ Maryland, Joint Ctr Astrophys, CRESST, Baltimore, MD 21250 USA. [Ramirez-Ruiz, E.; Prochaska, J. X.] Univ Calif Santa Cruz, UCO Lick Observ, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA. [Levan, A. J.] Univ Warwick, Dept Phys, Coventry CV4 7AL, W Midlands, England. [Bunker, A.] Univ Exeter, Sch Phys, Exeter EX4 4QJ, Devon, England. [Bunker, A.] Anglo Australian Observ, Eastwood, NSW 2122, Australia. [Chen, H-W.] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA. [Glazebrook, K.] Swinburne Univ Technol, Hawthorn, Vic 3122, Australia. [Hall, P. B.] York Univ, Dept Phys & Astron, N York, ON M3J 1P3, Canada. [Hurley, K. C.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Kocevski, D.] Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, Menlo Pk, CA 94025 USA. [Lopez, S.] Univ Chile, Dept Astron, Santiago, Chile. [Norris, J.] Univ Denver, Dept Phys & Astron, Denver, CO 80208 USA. [Tanvir, N.] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England. RP Perley, DA (reprint author), Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. RI Gehrels, Neil/D-2971-2012; Glazebrook, Karl/N-3488-2015; Lopez, Sebastian /I-5657-2016 OI Glazebrook, Karl/0000-0002-3254-9044; Lopez, Sebastian /0000-0003-0389-0902 FU NASA/Swift Guest Investigator [NNG05GF55G, NNG05GO22H]; NSF-DOE [PHY-0812811]; Royal Society Wolfson Research Merit Award; US Department of Energy [DEFC02-06ER41453]; NSF [AST-0607485]; TABASGO Foundation; NASA [Swift NX07AE98G]; DOE SciDAC [DEFC02- 01ER41176]; W.M. Keck Foundation FX J.S.B.'s group is supported in part by the Hellman Faculty Fund, Las Cumbres Observatory Global Telescope Network, and NASA/Swift Guest Investigator grant NNG05GF55G. B. M. and E. Q. were supported in part by the David and Lucile Packard Foundation, NASA grant NNG05GO22H, and the NSF-DOE Grant PHY-0812811. J. G. gratefully acknowledges a Royal Society Wolfson Research Merit Award. N.R.B. is partially supported by US Department of Energy SciDAC grant DEFC02-06ER41453 and by a NASA GLAST/Fermi Fellowship. A. V. F. is partially supported by NSF grant AST-0607485 and the TABASGO Foundation. This work was supported in part by NASA (Swift NX07AE98G, ER-R) and DOE SciDAC (DEFC02- 01ER41176, ER-R).; This research is based in part on observations obtained at the Gemini Observatory, which is operated by the Association of Universities for Research in Astronomy, Inc., under a cooperative agreement with the NSF on behalf of the Gemini partnership. Some of the data presented herein were obtained at the W. M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California, and the National Aeronautics and Space Administration (NASA). The Observatory was made possible by the generous financial support of the W.M. Keck Foundation. NR 117 TC 78 Z9 80 U1 1 U2 7 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 MAY 10 PY 2009 VL 696 IS 2 BP 1871 EP 1885 DI 10.1088/0004-637X/696/2/1871 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 441IO UT WOS:000265762700069 ER PT J AU Boden, AF Akeson, RL Sargent, AI Carpenter, JM Ciardi, DR Bary, JS Skrutskie, MF AF Boden, Andrew F. Akeson, Rachel L. Sargent, Anneila I. Carpenter, John M. Ciardi, David R. Bary, Jeffrey S. Skrutskie, Michael F. TI INTERFEROMETRIC EVIDENCE FOR RESOLVED WARM DUST IN THE DQ TAU SYSTEM SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE binaries: spectroscopic; circumstellar matter; stars: individual (DQ Tau); stars: pre-main sequence ID MAIN-SEQUENCE STARS; CLASSICAL T TAURI; PRELIMINARY PHYSICAL ORBIT; SPECTROSCOPIC BINARIES; DYNAMICAL MASSES; EMISSION; DISK; CIRCUMSTELLAR; ACCRETION; LIGHT AB We report on near-infrared (IR) interferometric observations of the double-lined pre-main sequence binary system DQ Tau. We model these data with a visual orbit for DQ Tau supported by the spectroscopic orbit and analysis of Mathieu et al. Further, DQ Tau exhibits significant near-IR excess; modeling our data requires inclusion of near-IR light from an "excess" source. Remarkably, the excess source is resolved in our data, similar in scale to the binary itself (similar to 0.2 AU at apastron), rather than the larger circumbinary disk (similar to 0.4 AU radius). Our observations support the Mathieu et al. and Carr et al. inference of significant warm material near the DQ Tau binary. C1 [Boden, Andrew F.; Sargent, Anneila I.; Carpenter, John M.] CALTECH, Div Phys Math & Astron, Pasadena, CA 91125 USA. [Boden, Andrew F.; Akeson, Rachel L.; Ciardi, David R.] CALTECH, NASA, Exoplanet Sci Inst, Pasadena, CA 91125 USA. [Bary, Jeffrey S.] Colgate Univ, Dept Phys & Astron, Hamilton, NY 13346 USA. [Skrutskie, Michael F.] Univ Virginia, Dept Astron, Charlottesville, VA 22903 USA. RP Boden, AF (reprint author), CALTECH, Div Phys Math & Astron, MS 105-24, Pasadena, CA 91125 USA. EM bode@astro.caltech.edu OI Akeson, Rachel/0000-0001-9674-1564; Ciardi, David/0000-0002-5741-3047 NR 23 TC 20 Z9 20 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD MAY 10 PY 2009 VL 696 IS 2 BP L111 EP L114 DI 10.1088/0004-637X/696/2/L111 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 438BS UT WOS:000265531500001 ER PT J AU Liang, LS Di Girolamo, L Platnick, S AF Liang, Lusheng Di Girolamo, Larry Platnick, Steven TI View-angle consistency in reflectance, optical thickness and spherical albedo of marine water-clouds over the northeastern Pacific through MISR-MODIS fusion SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID HETEROGENEITY; DEPENDENCE AB View-angle consistency in bidirectional reflectance factor (BRF), optical thickness and spherical albedo is examined for marine water clouds over a region of the northeastern Pacific using six years of fused Moderate Resolution Imaging Spectroradiometer (MODIS) and Multiangle Imaging SpectroRadiometer (MISR) data. Consistency is quantified by the root-mean-square of relative differences between MISR-measured BRF and their plane-parallel values and variation of plane-parallel retrieved optical thickness and spherical albedo across multiple view-angles. Probability distribution functions of consistency show that, for example, these clouds are angularly consistent within 5% in BRF, optical thickness and spherical albedo 72.2%, 39.0% and 81.1% of the time, respectively. We relate angular consistency to the spatial variability of nadir-BRF, thus allowing us to potentially identify, with a prescribed confidence level, which MODIS microphysical retrievals within the MISR swath meet the plane-parallel assumption to within any desired range in view-angle consistency. Citation: Liang, L., L. Di Girolamo, and S. Platnick (2009), View-angle consistency in reflectance, optical thickness and spherical albedo of marine water-clouds over the northeastern Pacific through MISR-MODIS fusion, Geophys. Res. Lett., 36, L09811, doi: 10.1029/2008GL037124. 2 C1 [Liang, Lusheng; Di Girolamo, Larry] Univ Illinois, Dept Atmospher Sci, Urbana, IL 61801 USA. [Platnick, Steven] NASA, Goddard Space Flight Ctr, Atmospheres Lab, Greenbelt, MD 20771 USA. RP Liang, LS (reprint author), Univ Illinois, Dept Atmospher Sci, 105 S Gregory St, Urbana, IL 61801 USA. EM lliang4@atmos.uiuc.edu RI liang, lusheng/E-1538-2014; Platnick, Steven/J-9982-2014 OI Platnick, Steven/0000-0003-3964-3567 FU NASA Earth and Space Science Fellowship; NASA New Investigator Program in Earth Science award; MISR FX This work was supported by a NASA Earth and Space Science Fellowship and a NASA New Investigator Program in Earth Science award, both under Program Manager Ming-Ying Wei. Additional support from the MISR project through the Jet Propulsion Laboratory of the California Institute of Technology is also gratefully acknowledged. We also thank two anonymous reviewers for their insightful comments. The MISR data were obtained from NASA Langley Research Center Atmospheric Sciences Data Center. The MODIS data were obtained through the Level 1 and Atmosphere Archive and Distribution System of NASA Goddard Space Flight Center. NR 18 TC 15 Z9 15 U1 1 U2 9 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 EI 1944-8007 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD MAY 9 PY 2009 VL 36 AR L09811 DI 10.1029/2008GL037124 PG 5 WC Geosciences, Multidisciplinary SC Geology GA 443RY UT WOS:000265929300002 ER PT J AU Qu, TD Song, YT AF Qu, Tangdong Song, Y. Tony TI Mindoro Strait and Sibutu Passage transports estimated from satellite data SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID SOUTH CHINA; SULU SEA; TOPOGRAPHY; OCEANS AB This study investigates the Mindoro Strait and Sibutu Passage transports using remotely-sensed sea surface height (SSH) and ocean-bottom-pressure (OBP) data. The analysis reveals the existence of a persistent baroclinic pressure gradient that drives a deepwater overflow from the South China Sea into the Sulu Sea. The application of hydraulic theory combined with the "geostrophic control" formula yields a mean transport estimate of about 2.4 Sv (1 Sv = 10(6) m(3) s(-1)) through the Mindoro Strait and about 2.8 Sv through the Sibutu Passage. Most of this water enters the Sulu Sea through the bottom layer of the Mindoro Strait and exits the Sulu Sea in the upper layer of the Sibutu Passage. The analysis also provides the first satellite-based observational evidence on the seasonal and interannual variation of the Mindoro Strait and Sibutu Passage transports for the period from January 2004 to December 2007. Citation: Qu, T., and Y. T. Song (2009), Mindoro Strait and Sibutu Passage transports estimated from satellite data, Geophys. Res. Lett., 36, L09601, doi: 10.1029/2009GL037314. C1 [Qu, Tangdong] Univ Hawaii Manoa, Int Pacific Res Ctr, SOEST, Honolulu, HI 96822 USA. [Song, Y. Tony] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Qu, TD (reprint author), Univ Hawaii Manoa, Int Pacific Res Ctr, SOEST, 1680 East West Rd,POST Bldg 406H, Honolulu, HI 96822 USA. EM tangdong@hawaii.edu FU NSF [OCE-0623533]; NASA; JAMSTEC; NOAA FX T. Qu was supported by the NSF through grant OCE-0623533 and Y.T. Song carried out the research at the Jet Propulsion Laboratory, California Institute of Technology, under contract with the NASA. Additional support for T. Qu was provided by the JAMSTEC, the NOAA, and the NASA through their sponsorship of the International Pacific Research Center (IPRC). School of Ocean and Earth Science and Technology contribution and IPRC contribution. NR 20 TC 18 Z9 19 U1 0 U2 7 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 EI 1944-8007 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD MAY 9 PY 2009 VL 36 AR L09601 DI 10.1029/2009GL037314 PG 5 WC Geosciences, Multidisciplinary SC Geology GA 443RY UT WOS:000265929300004 ER PT J AU Li, J Carlson, BE Lacis, AA AF Li, Jing Carlson, Barbara E. Lacis, Andrew A. TI A study on the temporal and spatial variability of absorbing aerosols using Total Ozone Mapping Spectrometer and Ozone Monitoring Instrument Aerosol Index data SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID INTERANNUAL VARIABILITY; MINERAL DUST; TOMS; TRANSPORT; PARTICLES; EMISSIONS; RECORD; FUTURE; REGION; TREND AB Absorbing aerosols, especially mineral dust and black carbon, play key roles in climate change by absorbing solar radiation, heating the atmosphere, and contributing to global warming. In this paper, we first examine the consistency of the Aerosol Index (AI) product as measured by the Total Ozone Mapping Spectrometer (TOMS) and Ozone Monitoring Instrument (OMI) instruments and then analyze these AI data sets to investigate the temporal and spatial variability of UVabsorbing aerosols. In contrast to the trend in aerosol optical depth found in the advanced very high-resolution radiometer data, no obvious long-term trend in absorbing aerosols is observed from the time series of AI records. The comparison between the mean annual cycle in the two data sets shows that the cycles agree very well both globally and regionally, indicating a consistency between the AI products from TOMS and OMI. Varimax rotated Empirical Orthogonal Function (EOF) analysis of detrended, deseasonalized AI data proves to be successful in isolating major dust and biomass burning source regions, as well as dust transport. Finally, we find that large, individual events, such as the Kuwait oil fire and Australian smoke plum, are isolated in individual higher-order principal components. C1 [Li, Jing] Columbia Univ, Dept Earth & Environm Sci, New York, NY 10025 USA. [Li, Jing; Carlson, Barbara E.; Lacis, Andrew A.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA. RP Li, J (reprint author), Columbia Univ, Dept Earth & Environm Sci, 2880 Broadway,Room 536, New York, NY 10025 USA. EM jli@giss.nasa.gov RI Lacis, Andrew/D-4658-2012; Carlson, Barbara/D-8319-2012; Li, Jing/J-2397-2014 OI Li, Jing/0000-0002-0540-0412 NR 29 TC 24 Z9 25 U1 0 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 MAY 9 PY 2009 VL 114 AR D09213 DI 10.1029/2008JD011278 PG 9 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 443SI UT WOS:000265930500006 ER PT J AU Abdo, AA Ackermann, M Ajello, M Atwood, WB Axelsson, M Baldini, L Ballet, J Barbiellini, G Bastieri, D Battelino, M Baughman, BM Bechtol, K Bellazzini, R Berenji, B Blandford, RD Bloom, ED Bogaert, G Bonamente, E Borgland, AW Bregeon, J Brez, A Brigida, M Bruel, P Burnett, TH Caliandro, GA Cameron, RA Caraveo, PA Carlson, P Casandjian, JM Cecchi, C Charles, E Chekhtman, A Cheung, CC Chiang, J Ciprini, S Claus, R Cohen-Tanugi, J Cominsky, LR Conrad, J Cutini, S Dermer, CD de Angelis, A de Palma, F Digel, SW Di Bernardo, G Silva, EDE Drell, PS Dubois, R Dumora, D Edmonds, Y Farnier, C Favuzzi, C Focke, WB Frailis, M Fukazawa, Y Funk, S Fusco, P Gaggero, D Gargano, F Gasparrini, D Gehrels, N Germani, S Giebels, B Giglietto, N Giordano, F Glanzman, T Godfrey, G Grasso, D Grenier, IA Grondin, MH Grove, JE Guillemot, L Guiriec, S Hanabata, Y Harding, AK Hartman, RC Hayashida, M Hays, E Hughes, RE Johannesson, G Johnson, AS Johnson, RP Johnson, WN Kamae, T Katagiri, H Kataoka, J Kawai, N Kerr, M Knodlseder, J Kocevski, D Kuehn, F Kuss, M Lande, J Latronico, L Lemoine-Goumard, M Longo, F Loparco, F Lott, B Lovellette, MN Lubrano, P Madejski, GM Makeev, A Massai, MM Mazziotta, MN McConville, W McEnery, JE Meurer, C Michelson, PF Mitthumsiri, W Mizuno, T Moiseev, AA Monte, C Monzani, ME Moretti, E Morselli, A Moskalenko, IV Murgia, S Nolan, PL Norris, JP Nuss, E Ohsugi, T Omodei, N Orlando, E Ormes, JF Ozaki, M Paneque, D Panetta, JH Parent, D Pelassa, V Pepe, M Pesce-Rollins, M Piron, F Pohl, M Porter, TA Profumo, S Raino, S Rando, R Razzano, M Reimer, A Reimer, O Reposeur, T Ritz, S Rochester, LS Rodriguez, AY Romani, RW Roth, M Ryde, F Sadrozinski, HFW Sanchez, D Sander, A Saz Parkinson, PM Scargle, JD Schalk, TL Sellerholm, A Sgro, C Smith, DA Smith, PD Spandre, G Spinelli, P Starck, JL Stephens, TE Strickman, MS Strong, AW Suson, DJ Tajima, H Takahashi, H Takahashi, T Tanaka, T Thayer, JB Thayer, JG Thompson, DJ Tibaldo, L Tibolla, O Torres, DF Tosti, G Tramacere, A Uchiyama, Y Usher, TL Van Etten, A Vasileiou, V Vilchez, N Vitale, V Waite, AP Wallace, E Wang, P Winer, BL Wood, KS Ylinen, T Ziegler, M AF Abdo, A. A. Ackermann, M. Ajello, M. Atwood, W. B. Axelsson, M. Baldini, L. Ballet, J. Barbiellini, G. Bastieri, D. Battelino, M. Baughman, B. M. Bechtol, K. Bellazzini, R. Berenji, B. Blandford, R. D. Bloom, E. D. Bogaert, G. Bonamente, E. Borgland, A. W. Bregeon, J. Brez, A. Brigida, M. Bruel, P. Burnett, T. H. Caliandro, G. A. Cameron, R. A. Caraveo, P. A. Carlson, P. Casandjian, J. M. Cecchi, C. Charles, E. Chekhtman, A. Cheung, C. C. Chiang, J. Ciprini, S. Claus, R. Cohen-Tanugi, J. Cominsky, L. R. Conrad, J. Cutini, S. Dermer, C. D. de Angelis, A. de Palma, F. Digel, S. W. Di Bernardo, G. do Couto e Silva, E. Drell, P. S. Dubois, R. Dumora, D. Edmonds, Y. Farnier, C. Favuzzi, C. Focke, W. B. Frailis, M. Fukazawa, Y. Funk, S. Fusco, P. Gaggero, D. Gargano, F. Gasparrini, D. Gehrels, N. Germani, S. Giebels, B. Giglietto, N. Giordano, F. Glanzman, T. Godfrey, G. Grasso, D. Grenier, I. A. Grondin, M. -H. Grove, J. E. Guillemot, L. Guiriec, S. Hanabata, Y. Harding, A. K. Hartman, R. C. Hayashida, M. Hays, E. Hughes, R. E. Johannesson, G. Johnson, A. S. Johnson, R. P. Johnson, W. N. Kamae, T. Katagiri, H. Kataoka, J. Kawai, N. Kerr, M. Knoedlseder, J. Kocevski, D. Kuehn, F. Kuss, M. Lande, J. Latronico, L. Lemoine-Goumard, M. Longo, F. Loparco, F. Lott, B. Lovellette, M. N. Lubrano, P. Madejski, G. M. Makeev, A. Massai, M. M. Mazziotta, M. N. McConville, W. McEnery, J. E. Meurer, C. Michelson, P. F. Mitthumsiri, W. Mizuno, T. Moiseev, A. A. Monte, C. Monzani, M. E. Moretti, E. Morselli, A. Moskalenko, I. V. Murgia, S. Nolan, P. L. Norris, J. P. Nuss, E. Ohsugi, T. Omodei, N. Orlando, E. Ormes, J. F. Ozaki, M. Paneque, D. Panetta, J. H. Parent, D. Pelassa, V. Pepe, M. Pesce-Rollins, M. Piron, F. Pohl, M. Porter, T. A. Profumo, S. Raino, S. Rando, R. Razzano, M. Reimer, A. Reimer, O. Reposeur, T. Ritz, S. Rochester, L. S. Rodriguez, A. Y. Romani, R. W. Roth, M. Ryde, F. Sadrozinski, H. F. -W. Sanchez, D. Sander, A. Saz Parkinson, P. M. Scargle, J. D. Schalk, T. L. Sellerholm, A. Sgro, C. Smith, D. A. Smith, P. D. Spandre, G. Spinelli, P. Starck, J. -L. Stephens, T. E. Strickman, M. S. Strong, A. W. Suson, D. J. Tajima, H. Takahashi, H. Takahashi, T. Tanaka, T. Thayer, J. B. Thayer, J. G. Thompson, D. J. Tibaldo, L. Tibolla, O. Torres, D. F. Tosti, G. Tramacere, A. Uchiyama, Y. Usher, T. L. Van Etten, A. Vasileiou, V. Vilchez, N. Vitale, V. Waite, A. P. Wallace, E. Wang, P. Winer, B. L. Wood, K. S. Ylinen, T. Ziegler, M. TI Measurement of the Cosmic Ray e(+)+e(-) Spectrum from 20 GeV to 1 TeV with the Fermi Large Area Telescope SO PHYSICAL REVIEW LETTERS LA English DT Article ID SUPERNOVA-REMNANTS; GAMMA-RAYS; ELECTRONS; ENERGIES AB Designed as a high-sensitivity gamma-ray observatory, the Fermi Large Area Telescope is also an electron detector with a large acceptance exceeding 2 m(2) sr at 300 GeV. Building on the gamma-ray analysis, we have developed an efficient electron detection strategy which provides sufficient background rejection for measurement of the steeply falling electron spectrum up to 1 TeV. Our high precision data show that the electron spectrum falls with energy as E-3.0 and does not exhibit prominent spectral features. Interpretations in terms of a conventional diffusive model as well as a potential local extra component are briefly discussed. C1 [Abdo, A. A.] CNR, Ottawa, ON, Canada. [Abdo, A. A.; Chekhtman, A.; Dermer, C. D.; Grove, J. E.; Johnson, W. N.; Lovellette, M. N.; Makeev, A.; Strickman, M. S.; Wood, K. S.] USN, Res Lab, Div Space Sci, Washington, DC 20375 USA. [Ackermann, M.; Ajello, M.; Bechtol, K.; Berenji, B.; Blandford, R. D.; Bloom, E. D.; Borgland, A. W.; Cameron, R. A.; Charles, E.; Chiang, J.; Claus, R.; Digel, S. W.; do Couto e Silva, E.; Drell, P. S.; Dubois, R.; Edmonds, Y.; Focke, W. B.; Funk, S.; Glanzman, T.; Godfrey, G.; Hayashida, M.; Johannesson, G.; Johnson, A. S.; Kamae, T.; Kocevski, D.; Lande, J.; Madejski, G. M.; Michelson, P. F.; Mitthumsiri, W.; Monzani, M. E.; Moskalenko, I. V.; Murgia, S.; Nolan, P. L.; Paneque, D.; Panetta, J. H.; Reimer, A.; Reimer, O.; Rochester, L. S.; Romani, R. W.; Tajima, H.; Tanaka, T.; Thayer, J. B.; Thayer, J. G.; Tramacere, A.; Uchiyama, Y.; Usher, T. L.; Van Etten, A.; Waite, A. P.; Wang, P.] Stanford Univ, WW Hansen Expt Phys Lab, Kavli Inst Particle Astrophys & Cosmol, Dept Phys, Stanford, CA 94305 USA. [Ackermann, M.; Ajello, M.; Bechtol, K.; Berenji, B.; Blandford, R. D.; Bloom, E. D.; Borgland, A. W.; Cameron, R. A.; Charles, E.; Chiang, J.; Claus, R.; Digel, S. W.; do Couto e Silva, E.; Drell, P. S.; Dubois, R.; Edmonds, Y.; Focke, W. B.; Funk, S.; Glanzman, T.; Godfrey, G.; Hayashida, M.; Johannesson, G.; Johnson, A. S.; Kamae, T.; Kocevski, D.; Lande, J.; Madejski, G. M.; Michelson, P. F.; Mitthumsiri, W.; Monzani, M. E.; Moskalenko, I. V.; Murgia, S.; Nolan, P. L.; Paneque, D.; Panetta, J. H.; Reimer, A.; Reimer, O.; Rochester, L. S.; Romani, R. W.; Tajima, H.; Tanaka, T.; Thayer, J. B.; Thayer, J. G.; Tramacere, A.; Uchiyama, Y.; Usher, T. L.; Van Etten, A.; Waite, A. P.; Wang, P.] Stanford Univ, SLAC Natl Accelerator Lab, Stanford, CA 94305 USA. [Atwood, W. B.; Johnson, R. P.; Porter, T. A.; Profumo, S.; Sadrozinski, H. F. -W.; Saz Parkinson, P. M.; Schalk, T. L.; Ziegler, M.] Univ Calif Santa Cruz, Santa Cruz Inst Particle Phys, Dept Phys, Santa Cruz, CA 95064 USA. [Atwood, W. B.; Johnson, R. P.; Porter, T. A.; Profumo, S.; Sadrozinski, H. F. -W.; Saz Parkinson, P. M.; Schalk, T. L.; Ziegler, M.] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA. [Axelsson, M.; Battelino, M.; Carlson, P.; Conrad, J.; Meurer, C.; Ryde, F.; Sellerholm, A.; Ylinen, T.] Oskar Klein Ctr Cosmo Particle Phys, SE-10691 Stockholm, Sweden. [Axelsson, M.] Stockholm Univ, Dept Astron, SE-10691 Stockholm, Sweden. [Baldini, L.; Bellazzini, R.; Bregeon, J.; Brez, A.; Di Bernardo, G.; Gaggero, D.; Grasso, D.; Kuss, M.; Latronico, L.; Massai, M. M.; Omodei, N.; Pesce-Rollins, M.; Razzano, M.; Sgro, C.; Spandre, G.] Ist Nazl Fis Nucl, Sez Pisa, I-56127 Pisa, Italy. [Ballet, J.; Casandjian, J. M.; Grenier, I. A.; Starck, J. -L.] Univ Paris Diderot, CEA Saclay, Lab AIM, CEA IRFU CNRS,Serv Astrophys, F-91191 Gif Sur Yvette, France. [Barbiellini, G.; Longo, F.; Moretti, E.] Ist Nazl Fis Nucl, Sez Trieste, I-34127 Trieste, Italy. [Barbiellini, G.; Longo, F.; Moretti, E.] Univ Trieste, Dipartimento Fis, I-34127 Trieste, Italy. [Bastieri, D.; Rando, R.; Tibaldo, L.] Ist Nazl Fis Nucl, Sez Padova, I-35131 Padua, Italy. [Bastieri, D.; Rando, R.; Tibaldo, L.] Univ Padua, Dipartimento Fis G Galilei, I-35131 Padua, Italy. [Battelino, M.; Carlson, P.; Conrad, J.; Ryde, F.; Ylinen, T.] Royal Inst Technol KTH, Dept Phys, SE-10691 Stockholm, Sweden. [Baughman, B. M.; Hughes, R. E.; Kuehn, F.; Sander, A.; Smith, P. D.; Winer, B. L.] Ohio State Univ, Dept Phys, Ctr Cosmol & Astroparticle Phys, Columbus, OH 43210 USA. [Bogaert, G.; Bruel, P.; Giebels, B.; Sanchez, D.] Ecole Polytech, CNRS, IN2P3, Lab Leprince Ringuet, F-91128 Palaiseau, France. [Bonamente, E.; Cecchi, C.; Ciprini, S.; Germani, S.; Lubrano, P.; Pepe, M.; Tosti, G.] Ist Nazl Fis Nucl, Sez Perugia, I-06123 Perugia, Italy. [Bonamente, E.; Cecchi, C.; Ciprini, S.; Germani, S.; Lubrano, P.; Pepe, M.; Tosti, G.] Univ Perugia, Dipartimento Fis, I-06123 Perugia, Italy. [Brigida, M.; Caliandro, G. A.; de Palma, F.; Favuzzi, C.; Fusco, P.; Giglietto, N.; Giordano, F.; Loparco, F.; Monte, C.; Raino, S.; Spinelli, P.] M Merlin Univ, Dipartimento Fis, I-70126 Bari, Italy. [Brigida, M.; Caliandro, G. A.; de Palma, F.; Favuzzi, C.; Fusco, P.; Gargano, F.; Giglietto, N.; Giordano, F.; Loparco, F.; Mazziotta, M. N.; Monte, C.; Raino, S.; Spinelli, P.] Ist Nazl Fis Nucl, Sez Bari, I-70126 Bari, Italy. [Burnett, T. H.; Kerr, M.; Roth, M.; Wallace, E.] Univ Washington, Dept Phys, Seattle, WA 98195 USA. [Brigida, M.; Caliandro, G. A.; de Palma, F.; Favuzzi, C.; Fusco, P.; Giglietto, N.; Giordano, F.; Loparco, F.; Monte, C.; Raino, S.; Spinelli, P.] Politecn Bari, I-70126 Bari, Italy. [Caraveo, P. A.] INAF Ist Astrofis Spaziale & Fis Cosm, I-20133 Milan, Italy. [Chekhtman, A.; Makeev, A.] George Mason Univ, Fairfax, VA 22030 USA. [Cheung, C. C.; Gehrels, N.; Harding, A. K.; Hartman, R. C.; Hays, E.; McConville, W.; McEnery, J. E.; Ritz, S.; Stephens, T. E.; Thompson, D. J.; Vasileiou, V.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Cohen-Tanugi, J.; Farnier, C.; Nuss, E.; Pelassa, V.; Piron, F.] Univ Montpellier 2, CNRS, IN2P3, Lab Phys Theor & Astroparticules, Montpellier, France. [Cominsky, L. R.] Sonoma State Univ, Dept Phys & Astron, Rohnert Pk, CA 94928 USA. [Conrad, J.; Meurer, C.; Sellerholm, A.] Stockholm Univ, Dept Phys, SE-10691 Stockholm, Sweden. [Cutini, S.; Gasparrini, D.] ASI, Sci Data Ctr, I-00044 Frascati, Roma, Italy. [de Angelis, A.; Frailis, M.] Univ Udine, Dipartimento Fis, I-33100 Udine, Italy. [de Angelis, A.; Frailis, M.] Ist Nazl Fis Nucl, Sez Trieste, Grp Collegato Udine, I-33100 Udine, Italy. [Dumora, D.; Grondin, M. -H.; Guillemot, L.; Lemoine-Goumard, M.; Lott, B.; Norris, J. P.; Parent, D.; Reposeur, T.; Smith, D. A.] Ctr Etud Nucl Bordeaux Gradignan, CNRS, IN2P3, UMR 5797, F-33175 Gradignan, France. [Dumora, D.; Grondin, M. -H.; Guillemot, L.; Lemoine-Goumard, M.; Lott, B.; Norris, J. P.; Parent, D.; Reposeur, T.; Smith, D. A.] Univ Bordeaux, Ctr Etud Nucl Bordeaux Gradignan, UMR 5797, F-33175 Gradignan, France. [Fukazawa, Y.; Hanabata, Y.; Katagiri, H.; Mizuno, T.; Ohsugi, T.; Takahashi, H.] Hiroshima Univ, Dept Phys Sci, Hiroshima 7398526, Japan. [Gehrels, N.; McConville, W.; Moiseev, A. A.; Ritz, S.] Univ Maryland, College Pk, MD 20742 USA. [Guiriec, S.] Univ Alabama, Huntsville, AL 35899 USA. [Kataoka, J.] Waseda Univ, Shinjuku Ku, Tokyo 1698050, Japan. [Kawai, N.] RIKEN, Cosm Radiat Lab, Inst Phys & Chem Res, Wako, Saitama 3510198, Japan. [Kawai, N.] Tokyo Inst Technol, Dept Phys, Meguro, Tokyo 1528551, Japan. [Knoedlseder, J.; Vilchez, N.] CNRS UPS, Ctr Etud Spatiale Rayonnements, F-31028 Toulouse 4, France. [Moiseev, A. A.] NASA, Goddard Space Flight Ctr, CRESST, Greenbelt, MD 20771 USA. [Morselli, A.; Vitale, V.] Ist Nazl Fis Nucl, Sez Roma Tor Vergata, I-00133 Rome, Italy. [Ormes, J. F.] Univ Denver, Dept Phys & Astron, Denver, CO 80208 USA. [Orlando, E.; Strong, A. W.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Ozaki, M.; Takahashi, T.] JAXA, Inst Space & Astronaut Sci, Sagamihara, Kanagawa 2298510, Japan. [Pohl, M.] Iowa State Univ, Dept Phys & Astron, Ames, IA 50011 USA. [Rodriguez, A. Y.; Torres, D. F.] CSIC, IEEC, Inst Ciencies Espai, Barcelona 08193, Spain. [Scargle, J. D.] NASA, Ames Res Ctr, Div Space Sci, Moffett Field, CA 94035 USA. [Suson, D. J.] Purdue Univ Calumet, Dept Chem & Phys, Hammond, IN 46323 USA. [Tibolla, O.] Max Planck Inst Kernphys, D-69029 Heidelberg, Germany. [Torres, D. F.] ICREA, Barcelona, Spain. [Tramacere, A.] CIFS, I-10133 Turin, Italy. [Vasileiou, V.] Univ Maryland, Baltimore, MD 21250 USA. [Vitale, V.] Univ Roma Tor Vergata, Dipartimento Fis, I-00133 Rome, Italy. [Ylinen, T.] Univ Kalmar, Sch Pure & Appl Nat Sci, SE-39182 Kalmar, Sweden. RP Abdo, AA (reprint author), CNR, Ottawa, ON, Canada. EM luca.latronico@pi.infn.it; Alexander.A.Moiseev@nasa.gov RI Kuss, Michael/H-8959-2012; lubrano, pasquale/F-7269-2012; Morselli, Aldo/G-6769-2011; Ozaki, Masanobu/K-1165-2013; Rando, Riccardo/M-7179-2013; Hays, Elizabeth/D-3257-2012; Johnson, Neil/G-3309-2014; Reimer, Olaf/A-3117-2013; Funk, Stefan/B-7629-2015; Loparco, Francesco/O-8847-2015; Johannesson, Gudlaugur/O-8741-2015; Gargano, Fabio/O-8934-2015; Moskalenko, Igor/A-1301-2007; Starck, Jean-Luc/D-9467-2011; Thompson, David/D-2939-2012; Harding, Alice/D-3160-2012; Gehrels, Neil/D-2971-2012; McEnery, Julie/D-6612-2012; Baldini, Luca/E-5396-2012; Nolan, Patrick/A-5582-2009; Grasso, Dario/I-2440-2012; giglietto, nicola/I-8951-2012; Tosti, Gino/E-9976-2013; Saz Parkinson, Pablo Miguel/I-7980-2013; Mazziotta, Mario /O-8867-2015; Sgro, Carmelo/K-3395-2016; Torres, Diego/O-9422-2016; Orlando, E/R-5594-2016; OI lubrano, pasquale/0000-0003-0221-4806; Morselli, Aldo/0000-0002-7704-9553; Reimer, Olaf/0000-0001-6953-1385; Funk, Stefan/0000-0002-2012-0080; Loparco, Francesco/0000-0002-1173-5673; Johannesson, Gudlaugur/0000-0003-1458-7036; Gargano, Fabio/0000-0002-5055-6395; Moskalenko, Igor/0000-0001-6141-458X; Starck, Jean-Luc/0000-0003-2177-7794; Thompson, David/0000-0001-5217-9135; Grasso, Dario/0000-0001-7761-7242; giglietto, nicola/0000-0002-9021-2888; Pesce-Rollins, Melissa/0000-0003-1790-8018; Cutini, Sara/0000-0002-1271-2924; Berenji, Bijan/0000-0002-4551-772X; Gasparrini, Dario/0000-0002-5064-9495; Tramacere, Andrea/0000-0002-8186-3793; Baldini, Luca/0000-0002-9785-7726; Mazziotta, Mario /0000-0001-9325-4672; Torres, Diego/0000-0002-1522-9065; Rando, Riccardo/0000-0001-6992-818X; Stephens, Thomas/0000-0003-3065-6871; Sgro', Carmelo/0000-0001-5676-6214; De Angelis, Alessandro/0000-0002-3288-2517; Frailis, Marco/0000-0002-7400-2135; Caraveo, Patrizia/0000-0003-2478-8018; Bastieri, Denis/0000-0002-6954-8862; Omodei, Nicola/0000-0002-5448-7577 FU NASA; DOE; CEA/Irfu and IN2P3/CNRS in France; ASI; INFN; MEXT; KEK; JAXA in Japan; K.A. Wallenberg Foundation; Swedish Research Council; National Space Board in Sweden FX The Fermi LAT Collaboration acknowledges support from a number of agencies and institutes for development and the operation of the LAT as well as scientific data analysis. These include NASA and DOE in the United States, CEA/Irfu and IN2P3/CNRS in France, ASI, INFN and INAF in Italy, MEXT, KEK, and JAXA in Japan, and the K.A. Wallenberg Foundation, the Swedish Research Council, and the National Space Board in Sweden. NR 28 TC 690 Z9 700 U1 1 U2 22 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 0031-9007 EI 1079-7114 J9 PHYS REV LETT JI Phys. Rev. Lett. PD MAY 8 PY 2009 VL 102 IS 18 AR 181101 DI 10.1103/PhysRevLett.102.181101 PG 6 WC Physics, Multidisciplinary SC Physics GA 443ZF UT WOS:000265948600011 PM 19518855 ER PT J AU Ando, M Kawamura, S Sato, S Nakamura, T Tsubono, K Araya, A Funaki, I Ioka, K Kanda, N Moriwaki, S Musha, M Nakazawa, K Numata, K Sakai, S Seto, N Takashima, T Tanaka, T Agatsuma, K Aoyanagi, KS Arai, K Asada, H Aso, Y Chiba, T Ebisuzaki, T Ejiri, Y Enoki, M Eriguchi, Y Fujimoto, MK Fujita, R Fukushima, M Futamase, T Ganzu, K Harada, T Hashimoto, T Hayama, K Hikida, W Himemoto, Y Hirabayashi, H Hiramatsu, T Hong, FL Horisawa, H Hosokawa, M Ichiki, K Ikegami, T Inoue, KT Ishidoshiro, K Ishihara, H Ishikawa, T Ishizaki, H Ito, H Itoh, Y Kawashima, N Kawazoe, F Kishimoto, N Kiuchi, K Kobayashi, S Kohri, K Koizumi, H Kojima, Y Kokeyama, K Kokuyama, W Kotake, K Kozai, Y Kudoh, H Kunimori, H Kuninaka, H Kuroda, K Maeda, KI Matsuhara, H Mino, Y Miyakawa, O Miyoki, S Morimoto, MY Morioka, T Morisawa, T Mukohyama, S Nagano, S Naito, I Nakamura, K Nakano, H Nakao, K Nakasuka, S Nakayama, Y Nishida, E Nishiyama, K Nishizawa, A Niwa, Y Noumi, T Obuchi, Y Ohashi, M Ohishi, N Ohkawa, M Okada, N Onozato, K Oohara, K Sago, N Saijo, M Sakagami, M Sakata, S Sasaki, M Sato, T Shibata, M Shinkai, H Somiya, K Sotani, H Sugiyama, N Suwa, Y Suzuki, R Tagoshi, H Takahashi, F Takahashi, K Takahashi, K Takahashi, R Takahashi, R Takahashi, T Takahashi, H Akiteru, T Takano, T Taniguchi, K Taruya, A Tashiro, H Torii, Y Toyoshima, M Tsujikawa, S Tsunesada, Y Ueda, A Ueda, K Utashima, M Wakabayashi, Y Yamakawa, H Yamamoto, K Yamazaki, T Yokoyama, J Yoo, CM Yoshida, S Yoshino, T AF Ando, Masaki Kawamura, Seiji Sato, Shuichi Nakamura, Takashi Tsubono, Kimio Araya, Akito Funaki, Ikkoh Ioka, Kunihito Kanda, Nobuyuki Moriwaki, Shigenori Musha, Mitsuru Nakazawa, Kazuhiro Numata, Kenji Sakai, Shin-ichiro Seto, Naoki Takashima, Takeshi Tanaka, Takahiro Agatsuma, Kazuhiro Aoyanagi, Koh-suke Arai, Koji Asada, Hideki Aso, Yoichi Chiba, Takeshi Ebisuzaki, Toshikazu Ejiri, Yumiko Enoki, Motohiro Eriguchi, Yoshiharu Fujimoto, Masa-Katsu Fujita, Ryuichi Fukushima, Mitsuhiro Futamase, Toshifumi Ganzu, Katsuhiko Harada, Tomohiro Hashimoto, Tatsuaki Hayama, Kazuhiro Hikida, Wataru Himemoto, Yoshiaki Hirabayashi, Hisashi Hiramatsu, Takashi Hong, Feng-Lei Horisawa, Hideyuki Hosokawa, Mizuhiko Ichiki, Kiyotomo Ikegami, Takeshi Inoue, Kaiki T. Ishidoshiro, Koji Ishihara, Hideki Ishikawa, Takehiko Ishizaki, Hideharu Ito, Hiroyuki Itoh, Yousuke Kawashima, Nobuki Kawazoe, Fumiko Kishimoto, Naoko Kiuchi, Kenta Kobayashi, Shiho Kohri, Kazunori Koizumi, Hiroyuki Kojima, Yasufumi Kokeyama, Keiko Kokuyama, Wataru Kotake, Kei Kozai, Yoshihide Kudoh, Hideaki Kunimori, Hiroo Kuninaka, Hitoshi Kuroda, Kazuaki Maeda, Kei-ichi Matsuhara, Hideo Mino, Yasushi Miyakawa, Osamu Miyoki, Shinji Morimoto, Mutsuko Y. Morioka, Tomoko Morisawa, Toshiyuki Mukohyama, Shinji Nagano, Shigeo Naito, Isao Nakamura, Kouji Nakano, Hiroyuki Nakao, Kenichi Nakasuka, Shinichi Nakayama, Yoshinori Nishida, Erina Nishiyama, Kazutaka Nishizawa, Atsushi Niwa, Yoshito Noumi, Taiga Obuchi, Yoshiyuki Ohashi, Masatake Ohishi, Naoko Ohkawa, Masashi Okada, Norio Onozato, Kouji Oohara, Kenichi Sago, Norichika Saijo, Motoyuki Sakagami, Masaaki Sakata, Shihori Sasaki, Misao Sato, Takashi Shibata, Masaru Shinkai, Hisaaki Somiya, Kentaro Sotani, Hajime Sugiyama, Naoshi Suwa, Yudai Suzuki, Rieko Tagoshi, Hideyuki Takahashi, Fuminobu Takahashi, Kakeru Takahashi, Keitaro Takahashi, Ryutaro Takahashi, Ryuichi Takahashi, Tadayuki Takahashi, Hirotaka Akiteru, Takamori Takano, Tadashi Taniguchi, Keisuke Taruya, Atsushi Tashiro, Hiroyuki Torii, Yasuo Toyoshima, Morio Tsujikawa, Shinji Tsunesada, Yoshiki Ueda, Akitoshi Ueda, Ken-ichi Utashima, Masayoshi Wakabayashi, Yaka Yamakawa, Hiroshi Yamamoto, Kazuhiro Yamazaki, Toshitaka Yokoyama, Jun'ichi Yoo, Chul-Moon Yoshida, Shijun Yoshino, Taizoh TI DECIGO pathfinder SO CLASSICAL AND QUANTUM GRAVITY LA English DT Article; Proceedings Paper CT 7th International LISA Symposium CY JUN 16-20, 2008 CL Barcelona, SPAIN SP LISA Int Sci Team, Inst Estudis Espacials Catalunya AB DECIGO pathfinder (DPF) is a milestone satellite mission for DECIGO (DECi-hertz Interferometer Gravitational wave Observatory), which is a future space gravitational wave antenna. DECIGO is expected to provide fruitful insights into the universe, particularly about dark energy, the formation mechanism of supermassive black holes and the inflation of the universe. Since DECIGO will be an extremely challenging mission, which will be formed by three drag-free spacecraft with 1000 km separation, it is important to increase the technical feasibility of DECIGO before its planned launch in 2024. Thus, we are planning to launch two milestone missions: DPF and pre-DECIGO. In this paper, we review the conceptual design and current status of the first milestone mission, DPF. C1 [Ando, Masaki; Tsubono, Kimio; Nakazawa, Kazuhiro; Agatsuma, Kazuhiro; Ichiki, Kiyotomo; Ishidoshiro, Koji; Kokuyama, Wataru; Kudoh, Hideaki; Morioka, Tomoko; Onozato, Kouji; Suwa, Yudai; Takahashi, Kakeru; Taruya, Atsushi; Yokoyama, Jun'ichi] Univ Tokyo, Dept Phys, Tokyo 1130033, Japan. [Kawamura, Seiji; Seto, Naoki; Arai, Koji; Ishizaki, Hideharu; Kotake, Kei; Nakamura, Kouji; Obuchi, Yoshiyuki; Ohishi, Naoko; Okada, Norio; Sakata, Shihori; Torii, Yasuo; Ueda, Akitoshi; Yamazaki, Toshitaka] Natl Astron Observ Japan, Tokyo 1818588, Japan. [Sato, Shuichi] Hosei Univ, Fac Engn, Tokyo 1848584, Japan. [Nakamura, Takashi; Ganzu, Katsuhiko; Morisawa, Toshiyuki; Tashiro, Hiroyuki] Kyoto Univ, Dept Phys, Kyoto 6068502, Japan. [Araya, Akito; Akiteru, Takamori] Univ Tokyo, Earthquake Res Inst, Tokyo 1130032, Japan. [Funaki, Ikkoh; Sakai, Shin-ichiro; Takashima, Takeshi; Hashimoto, Tatsuaki; Ishikawa, Takehiko; Kishimoto, Naoko; Koizumi, Hiroyuki; Kuninaka, Hitoshi; Matsuhara, Hideo; Morimoto, Mutsuko Y.; Nishiyama, Kazutaka; Takahashi, Tadayuki] Japan Aerosp Explorat Agcy, Inst Space & Astronaut Sci, Kanagawa 2298510, Japan. [Ioka, Kunihito] High Energy Accelerator Res Org, Inst Particle & Nucl Studies, Tsukuba, Ibaraki 3050801, Japan. [Ishihara, Hideki; Yoo, Chul-Moon] Osaka City Univ, Dept Phys, Osaka 5588585, Japan. [Kanda, Nobuyuki; Moriwaki, Shigenori] Univ Tokyo, Dept Adv Mat Sci, Chiba 2778561, Japan. [Musha, Mitsuru; Ueda, Ken-ichi] Univ Electrocommun, Inst Laser Sci, Tokyo 1828585, Japan. [Numata, Kenji] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Tanaka, Takahiro; Sasaki, Misao; Takahashi, Keitaro] Kyoto Univ, Yukawa Inst Theoret Phys, Kyoto 6068502, Japan. [Aoyanagi, Koh-suke; Kiuchi, Kenta; Maeda, Kei-ichi] Waseda Univ, Dept Phys, Tokyo 1698555, Japan. [Asada, Hideki] Hirosaki Univ, Dept Earth & Environm Sci, Aomori 0368560, Japan. [Aso, Yoichi; Mino, Yasushi; Miyakawa, Osamu; Somiya, Kentaro] CALTECH, Pasadena, CA 91125 USA. [Chiba, Takeshi] Nihon Univ, Setagaya Ku, Tokyo 1568550, Japan. [Ebisuzaki, Toshikazu] RIKEN, Wako, Saitama 3510198, Japan. [Ejiri, Yumiko; Kokeyama, Keiko; Nishida, Erina; Suzuki, Rieko] Ochanomizu Univ, Tokyo 1120012, Japan. [Enoki, Motohiro] Tokyo Keizai Univ, Fac Business Adm, Tokyo 1858502, Japan. [Eriguchi, Yoshiharu; Shibata, Masaru] Univ Tokyo, Dept Earth Sci & Astron, Tokyo 1538902, Japan. [Fujita, Ryuichi] Raman Res Inst, Bangalore 560080, Karnataka, India. [Futamase, Toshifumi; Yoshida, Shijun] Tohoku Univ, Astron Inst, Sendai, Miyagi 9808578, Japan. [Harada, Tomohiro] Rikkyo Univ, Dept Phys, Tokyo 1718501, Japan. [Hayama, Kazuhiro] Univ Texas Brownsville, Brownsville, TX 78520 USA. [Hikida, Wataru; Tagoshi, Hideyuki] Osaka Univ, Dept Earth & Space Sci, Osaka 5600043, Japan. [Himemoto, Yoshiaki] Shibaura Inst Technol, Ctr Educ Assistance, Saitama 3378570, Japan. [Hirabayashi, Hisashi] Japan Aerosp Explorat Agcy, Space Educ Ctr, Sagamihara, Kanagawa 2298510, Japan. [Hiramatsu, Takashi; Miyoki, Shinji; Ohashi, Masatake] Univ Tokyo, Inst Cosm Ray Res, Chiba 2778582, Japan. [Hong, Feng-Lei; Ikegami, Takeshi] Natl Inst Adv Ind Sci & Technol, Tsukuba 3058563, Japan. [Horisawa, Hideyuki] Tokai Univ, Dept Aeronaut & Astronaut, Kanagawa 2591292, Japan. [Hosokawa, Mizuhiko; Ito, Hiroyuki; Kunimori, Hiroo; Nagano, Shigeo; Toyoshima, Morio] Natl Inst Informat & Commun Technol, Koganei, Tokyo 1848795, Japan. [Inoue, Kaiki T.; Kawashima, Nobuki] Kinki Univ, Sch Sci & Engn, Osaka 5778502, Japan. [Itoh, Yousuke; Taniguchi, Keisuke] Univ Wisconsin, Dept Phys, Milwaukee, WI 53211 USA. [Kawazoe, Fumiko; Yamamoto, Kazuhiro] Max Planck Inst Gravitat Phys, Albert Einstein Inst, D-30167 Hannover, Germany. [Kobayashi, Shiho] Liverpool John Moores Univ, Astrophys Res Inst, Birkenhead L41 1LD, Merseyside, England. [Kohri, Kazunori] Univ Tubingen, Inst Astron & Astrophys, D-72076 Tubingen, Germany. [Kojima, Yasufumi] Hiroshima Univ, Grad Sch Sci, Hiroshima 7398526, Japan. [Kozai, Yoshihide; Kuroda, Kazuaki] Gunma Astron Observ, Gunma 3770702, Japan. [Mukohyama, Shinji; Takahashi, Fuminobu] Univ Tokyo, IPMU, Chiba 2778568, Japan. [Nakano, Hiroyuki] Rochester Inst Technol, Rochester, NY 14623 USA. [Nakasuka, Shinichi; Noumi, Taiga] Univ Tokyo, Dept Aeronaut & Astroaut, Tokyo 1138656, Japan. [Nakayama, Yoshinori] Natl Def Acad, Dept Aerosp Engn, Yokosuka, Kanagawa 2398686, Japan. [Nishizawa, Atsushi; Niwa, Yoshito; Sakagami, Masaaki] Kyoto Univ, Fac Intergrated Human Studies, Kyoto 6068501, Japan. [Ohkawa, Masashi; Oohara, Kenichi; Sato, Takashi] Niigata Univ, Niigata 9502181, Japan. [Saijo, Motoyuki] Rikkyo Univ, Dept Phys, Tokyo 1718501, Japan. [Shinkai, Hisaaki] Osaka Inst Technol, Dept Informat Syst, Hirakata, Osaka 5730196, Japan. [Sotani, Hajime] Univ Tubingen, Inst Astron & Astrophys, D-72076 Tubingen, Germany. [Sugiyama, Naoshi; Takahashi, Ryuichi] Nagoya Univ, Grad Sch Sci, Nagoya, Aichi 4648601, Japan. [Takahashi, Hirotaka] Nagaoka Univ Technol, Dept Management & Informat Syst Sci, Niigata 9402188, Japan. [Takano, Tadashi] Nihon Univ, Dept Elect & Comp Sci, Funabashi, Chiba 2748501, Japan. [Tsujikawa, Shinji] Tokyo Univ Sci, Dept Phys, Tokyo 1628601, Japan. [Tsunesada, Yoshiki] Tokyo Inst Technol, Grad Sch Sci & Engn Phys, Tokyo 1528550, Japan. [Utashima, Masayoshi] Japan Aerosp Explorat Agcy, Tsukuba Space Ctr, Tsukuba, Ibaraki 3058505, Japan. [Yamakawa, Hiroshi] Kyoto Univ, Res Inst Sustainable Humanosphere, Kyoto 6110011, Japan. RP Ando, M (reprint author), Kyoto Univ, Dept Phys, Kyoto 6068202, Japan. EM ando@granite.phys.s.u-tokyo.ac.jp RI Kawazoe, Fumiko/F-7700-2011; Chiba, Takeshi/G-3510-2011; Mukohyama, Shinji/A-4401-2011; Hong, Feng-Lei/N-3098-2014; M, Manjunath/N-4000-2014; Takahashi, Keitaro/L-5930-2015; Taniguchi, Keisuke/G-2694-2011; Takahashi, Ryuichi/F-3362-2013; Nakamura, Kouji/H-6364-2013; Suwa, Yudai/G-9711-2012; ANDO, MASAKI/G-4989-2014; OI Chiba, Takeshi/0000-0002-9737-2569; Hong, Feng-Lei/0000-0003-1318-2635; M, Manjunath/0000-0001-8710-0730; Nakamura, Kouji/0000-0001-6148-4289; ANDO, MASAKI/0000-0002-8865-9998; Nishizawa, Atsushi/0000-0003-3562-0990; Sasaki, Misao/0000-0001-5924-0664; Nakano, Hiroyuki/0000-0001-7665-0796 NR 9 TC 8 Z9 8 U1 0 U2 6 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0264-9381 EI 1361-6382 J9 CLASSICAL QUANT GRAV JI Class. Quantum Gravity PD MAY 7 PY 2009 VL 26 IS 9 AR 094019 DI 10.1088/0264-9381/26/9/094019 PG 9 WC Astronomy & Astrophysics; Physics, Multidisciplinary; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA 435NC UT WOS:000265349600020 ER PT J AU Arun, KG Babak, S Berti, E Cornish, N Cutler, C Gair, J Hughes, SA Iyer, BR Lang, RN Mandel, I Porter, EK Sathyaprakash, BS Sinha, S Sintes, AM Trias, M Van Den Broeck, C Volonteri, M AF Arun, K. G. Babak, Stas Berti, Emanuele Cornish, Neil Cutler, Curt Gair, Jonathan Hughes, Scott A. Iyer, Bala R. Lang, Ryan N. Mandel, Ilya Porter, Edward K. Sathyaprakash, Bangalore S. Sinha, Siddhartha Sintes, Alicia M. Trias, Miquel Van Den Broeck, Chris Volonteri, Marta TI Massive black-hole binary inspirals: results from the LISA parameter estimation taskforce SO CLASSICAL AND QUANTUM GRAVITY LA English DT Article; Proceedings Paper CT 7th International LISA Symposium CY JUN 16-20, 2008 CL Barcelona, SPAIN SP LISA Int Sci Team, Inst Estudis Espacials Catalunya ID GRAVITATIONAL WAVE-FORMS; STANDARD SIRENS; HIERARCHICAL-MODELS; GALAXY FORMATION; COMPACT OBJECTS; MERGERS; ACCRETION; EVOLUTION; COLLAPSE; SYSTEMS AB The LISA Parameter Estimation Taskforce was formed in September 2007 to provide the LISA Project with vetted codes, source distribution models and results related to parameter estimation. The Taskforce's goal is to be able to quickly calculate the impact of any mission design changes on LISA's science capabilities, based on reasonable estimates of the distribution of astrophysical sources in the universe. This paper describes our Taskforce's work on massive black-hole binaries (MBHBs). Given present uncertainties in the formation history of MBHBs, we adopt four different population models, based on (i) whether the initial black-hole seeds are small or large and (ii) whether accretion is efficient or inefficient at spinning up the holes. We compare four largely independent codes for calculating LISA's parameter-estimation capabilities. All codes are based on the Fisher-matrix approximation, but in the past they used somewhat different signal models, source parametrizations and noise curves. We show that once these differences are removed, the four codes give results in extremely close agreement with each other. Using a code that includes both spin precession and higher harmonics in the gravitational-wave signal, we carry out Monte Carlo simulations and determine the number of events that can be detected and accurately localized in our four population models. C1 [Arun, K. G.] Univ Paris 11, LAL, CNRS, IN2P3, Orsay, France. [Arun, K. G.] Univ Paris 06, Inst Astrophys Paris, UMR 7095, CNRS, F-75014 Paris, France. [Babak, Stas; Porter, Edward K.; Sintes, Alicia M.] Max Planck Inst Gravitat Phys, Albert Einstein Inst, D-14476 Golm, Germany. [Berti, Emanuele; Cutler, Curt] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Berti, Emanuele] Univ Mississippi, Dept Phys & Astron, University, MS 38677 USA. [Cornish, Neil] Montana State Univ, Dept Phys, Bozeman, MT 59717 USA. [Cutler, Curt] CALTECH, Pasadena, CA 91125 USA. [Gair, Jonathan] Univ Cambridge, Inst Astron, Cambridge CB30HA, England. [Hughes, Scott A.; Lang, Ryan N.] MIT, Dept Phys, Cambridge, MA 02139 USA. [Hughes, Scott A.; Lang, Ryan N.] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. [Iyer, Bala R.; Sinha, Siddhartha] Raman Res Inst, Bangalore 560080, Karnataka, India. [Mandel, Ilya] Northwestern Univ, Dept Phys & Astron, Evanston, IL USA. [Porter, Edward K.] APC, F-75205 Paris 13, France. [Sathyaprakash, Bangalore S.; Van Den Broeck, Chris] Cardiff Univ, Sch Phys & Astron, Cardiff CF24 3YB, S Glam, Wales. [Sinha, Siddhartha] Indian Inst Sci, Dept Phys, Bangalore 560012, Karnataka, India. [Sintes, Alicia M.; Trias, Miquel] Univ Illes Balears, Dept Fis, E-07122 Palma de Mallorca, Spain. [Volonteri, Marta] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. RP Arun, KG (reprint author), Univ Paris 11, LAL, CNRS, IN2P3, Orsay, France. RI Iyer, Bala R./E-2894-2012; M, Manjunath/N-4000-2014; Berti, Emanuele/C-9331-2016; OI Iyer, Bala R./0000-0002-4141-5179; M, Manjunath/0000-0001-8710-0730; Berti, Emanuele/0000-0003-0751-5130; Mandel, Ilya/0000-0002-6134-8946 NR 51 TC 69 Z9 69 U1 0 U2 4 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 MAY 7 PY 2009 VL 26 IS 9 AR 094027 DI 10.1088/0264-9381/26/9/094027 PG 14 WC Astronomy & Astrophysics; Physics, Multidisciplinary; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA 435NC UT WOS:000265349600028 ER PT J AU Livas, JC Thorpe, JI Numata, K Mitryk, S Mueller, G Wand, V AF Livas, J. C. Thorpe, J. I. Numata, K. Mitryk, S. Mueller, G. Wand, V. TI Frequency-tunable pre-stabilized lasers for LISA via sideband locking SO CLASSICAL AND QUANTUM GRAVITY LA English DT Article; Proceedings Paper CT 7th International LISA Symposium CY JUN 16-20, 2008 CL Barcelona, SPAIN SP LISA Int Sci Team, Inst Estudis Espacials Catalunya ID SPECTRAL-PURITY LASER; PHASE AB Laser frequency noise mitigation is one of the most challenging aspects of the LISA interferometric measurement system. The unstabilized frequency fluctuations must be suppressed by roughly 12 orders of magnitude in order to achieve stability sufficient for gravitational wave detection. This enormous suppression will be achieved through a combination of stabilization and common-mode rejection techniques. The stabilization component will itself be achieved in two stages: pre-stabilization to a local optical reference followed by arm locking to some combination of the inter-spacecraft distances. In order for these two stabilization stages to work simultaneously, the lock-point of the pre-stabilization loop must be frequency tunable. The current baseline stabilization technique, Pound-Drever-Hall locking to an optical cavity, does not provide tunability between cavity resonances. Here we present a modification to the baseline technique that allows the laser to be locked to a cavity resonance with an adjustable frequency offset. This technique requires no modifications to the optical cavity itself, thus preserving the stability of the frequency reference. We present measurements of the system performance and demonstrate that the offset locking techniques are compatible with arm locking. C1 [Livas, J. C.; Thorpe, J. I.; Numata, K.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Numata, K.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Mitryk, S.; Mueller, G.; Wand, V.] Univ Florida, Dept Phys, Gainesville, FL 32611 USA. RP Livas, JC (reprint author), NASA, Goddard Space Flight Ctr, 8800 Greenbelt Rd, Greenbelt, MD 20771 USA. EM Jeffrey.Livas@nasa.gov RI Livas, Jeffrey/D-2994-2012; Thorpe, James/D-3150-2012 NR 16 TC 11 Z9 11 U1 1 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0264-9381 J9 CLASSICAL QUANT GRAV JI Class. Quantum Gravity PD MAY 7 PY 2009 VL 26 IS 9 AR 094016 DI 10.1088/0264-9381/26/9/094016 PG 10 WC Astronomy & Astrophysics; Physics, Multidisciplinary; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA 435NC UT WOS:000265349600017 ER PT J AU Stebbins, RT AF Stebbins, R. T. TI Rightsizing LISA SO CLASSICAL AND QUANTUM GRAVITY LA English DT Article; Proceedings Paper CT 7th International LISA Symposium CY JUN 16-20, 2008 CL Barcelona, SPAIN SP LISA Int Sci Team, Inst Estudis Espacials Catalunya AB The Laser Interferometer Space Antenna (LISA) science requirements and conceptual design have been fairly stable for over a decade. In the interest of reducing costs, the LISA Project at NASA has looked for simplifications of the architecture, at downsizing of subsystems and at descopes of the entire mission. This is a natural activity of the formulation phase and one that is particularly timely in the current NASA budgetary context. There is, and will continue to be, enormous pressure for cost reduction from both ESA and NASA, reviewers and the broader research community. Here, the rationale for the baseline architecture is reviewed, and recent efforts to find simplifications and other reductions that might lead to savings are reported. A few possible simplifications have been found in the LISA baseline architecture. In the interest of exploring cost sensitivity, one moderate and one aggressive descope have been evaluated; the cost savings are modest and the loss of science is not. C1 NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Stebbins, RT (reprint author), NASA, Goddard Space Flight Ctr, Code 663, Greenbelt, MD 20771 USA. EM Robin.T.Stebbins@nasa.gov RI Stebbins, Robin/G-5009-2013 NR 7 TC 7 Z9 7 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0264-9381 J9 CLASSICAL QUANT GRAV JI Class. Quantum Gravity PD MAY 7 PY 2009 VL 26 IS 9 AR 094014 DI 10.1088/0264-9381/26/9/094014 PG 10 WC Astronomy & Astrophysics; Physics, Multidisciplinary; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA 435NC UT WOS:000265349600015 ER PT J AU Thorpe, JI McWilliams, ST Kelly, BJ Fahey, RP Arnaud, K Baker, JG AF Thorpe, J. I. McWilliams, S. T. Kelly, B. J. Fahey, R. P. Arnaud, K. Baker, J. G. TI LISA parameter estimation using numerical merger waveforms SO CLASSICAL AND QUANTUM GRAVITY LA English DT Article; Proceedings Paper CT 7th International LISA Symposium CY JUN 16-20, 2008 CL Barcelona, SPAIN SP LISA Int Sci Team, Inst Estudis Espacials Catalunya AB Recent advances in numerical relativity provide a detailed description of the waveforms of coalescing massive black hole binaries (MBHBs), expected to be the strongest detectable LISA sources. We present a preliminary study of LISA's sensitivity to MBHB parameters using a hybrid numerical/analytic waveform for equal-mass, non-spinning holes. The Synthetic LISA software package is used to simulate the instrument response, and the Fisher information matrix method is used to estimate errors in the parameters. Initial results indicate that inclusion of the merger signal can significantly improve the precision of some parameter estimates. For example, the median parameter errors for an ensemble of systems with total redshifted mass of 10(6)M(circle dot) at a redshift of z similar to 1 were found to decrease by a factor of slightly more than two for signals with merger as compared to signals truncated at the Schwarzchild ISCO. C1 [Thorpe, J. I.; McWilliams, S. T.; Kelly, B. J.; Fahey, R. P.; Arnaud, K.; Baker, J. G.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Arnaud, K.] Univ Maryland, CRESST, College Pk, MD 20742 USA. [Arnaud, K.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. RP Thorpe, JI (reprint author), NASA, Goddard Space Flight Ctr, 8800 Greenbelt Rd, Greenbelt, MD 20771 USA. EM James.I.Thorpe@nasa.gov RI Kelly, Bernard/G-7371-2011; Thorpe, James/D-3150-2012; OI Kelly, Bernard/0000-0002-3326-4454 NR 22 TC 10 Z9 10 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0264-9381 J9 CLASSICAL QUANT GRAV JI Class. Quantum Gravity PD MAY 7 PY 2009 VL 26 IS 9 AR 094026 DI 10.1088/0264-9381/26/9/094026 PG 10 WC Astronomy & Astrophysics; Physics, Multidisciplinary; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA 435NC UT WOS:000265349600027 ER PT J AU Vallisneri, M AF Vallisneri, Michele TI A LISA data-analysis primer SO CLASSICAL AND QUANTUM GRAVITY LA English DT Article; Proceedings Paper CT 7th International LISA Symposium CY JUN 16-20, 2008 CL Barcelona, SPAIN SP LISA Int Sci Team, Inst Estudis Espacials Catalunya ID GRAVITATIONAL-RADIATION; GALACTIC BINARIES; COMPACT BINARIES; INTERFEROMETER; WAVES AB This paper is an introduction for the nonpractitioner to the ideas and issues of LISA data analysis, as reflected in the explorations and experiments of the participants in the Mock LISA Data Challenges. In particular, I discuss the methods and codes that have been developed for the detection and parameter estimation of supermassive black-hole binaries, extreme mass-ratio inspirals and galactic binaries. C1 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 98 TC 7 Z9 7 U1 1 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0264-9381 EI 1361-6382 J9 CLASSICAL QUANT GRAV JI Class. Quantum Gravity PD MAY 7 PY 2009 VL 26 IS 9 AR 094024 DI 10.1088/0264-9381/26/9/094024 PG 12 WC Astronomy & Astrophysics; Physics, Multidisciplinary; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA 435NC UT WOS:000265349600025 ER PT J AU Houborg, R Anderson, MC AF Houborg, Rasmus Anderson, Martha C. TI Utility of an image-based canopy reflectance modeling tool for remote estimation of LAI and leaf chlorophyll content at regional scales SO JOURNAL OF APPLIED REMOTE SENSING LA English DT Article DE Leaf chlorophyll; LAI; radiative transfer; SPOT; Look-up table inversion; Regularization ID RADIATIVE-TRANSFER MODELS; VEGETATION BIOPHYSICAL PARAMETERS; AREA INDEX; SATELLITE DATA; MODIS DATA; ATMOSPHERIC CORRECTION; PRECISION AGRICULTURE; INVERSION METHODS; ENERGY FLUXES; WATER-CONTENT AB This paper describes a novel physically-based approach for estimating leaf area index (LAI) and leaf chlorophyll content (C(ab)) at regional scales that relies on radiance data acquirable from a suite of aircraft and operational satellite sensors. The REGularized canopy reFLECtance (REGFLEC) modeling tool integrates leaf optics (PROSPECT), canopy reflectance (ACRM), and atmospheric radiative transfer (6SV1) model components, facilitating the direct use of at-sensor radiances in green, red and near-infrared wavelengths. REGFLEC adopts a multi-step LUT-based inversion approach and incorporates image-based techniques to reduce the confounding effects of land cover specific vegetation parameters and soil reflectance. REGFLEC was applied to agricultural and natural vegetation areas using 10 m and 20 m resolution SPOT imagery, and variable environmental and plant development conditions allowed for model validation over a wide range in LAI (0-6) and C(ab) (20-75 mu g cm(-2)). Validation against in-situ measurements yielded relative root-mean-square deviations on the order of 13% (0.4) for LAI and between 11-19% (4.9-9.1 mu g cm(-2)) for C(ab). REGFLEC demonstrated good utility in detecting spatial and temporal variations in LAI and C(ab) without requiring site-specific data for calibration. The physical approach presented here can quite easily be applied to other regions and has the potential of being more universally applicable than traditional empirical approaches for retrieving LAI and C(ab). C1 [Houborg, Rasmus] Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20742 USA. [Houborg, Rasmus] NASA, Hydrol Sci Branch, Goddard Space Flight Ctr, Greenbelt, MD USA. [Anderson, Martha C.] ARS, USDA, Hydrol & Remote Sensing Lab, Beltsville, MD 20705 USA. RP Houborg, R (reprint author), Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20742 USA. EM Rasmus.Houborg@nasa.gov; Martha.Anderson@ars.usda.gov RI Anderson, Martha/C-1720-2015 OI Anderson, Martha/0000-0003-0748-5525 FU USDA Agricultural Research Service Research Associate Program FX Funding for this research was provided by the USDA Agricultural Research Service Research Associate Program. We would like to acknowledge Wayne Dulaney and Principal Investigator Brent Holben of the AERONET sites for making sun photometer data available. Trade names are included for the benefit of the reader and do not imply an endorsement of or a preference for the product listed by the U. S. Department of Agriculture. NR 74 TC 13 Z9 13 U1 0 U2 9 PU SPIE-SOC PHOTOPTICAL INSTRUMENTATION ENGINEERS PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98225 USA SN 1931-3195 J9 J APPL REMOTE SENS JI J. Appl. Remote Sens. PD MAY 7 PY 2009 VL 3 AR 033529 DI 10.1117/1.3141522 PG 29 WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic Technology SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science & Photographic Technology GA 520WK UT WOS:000271880000001 ER PT J AU McComiskey, A Feingold, G Frisch, AS Turner, DD Miller, MA Chiu, JC Min, QL Ogren, JA AF McComiskey, Allison Feingold, Graham Frisch, A. Shelby Turner, David D. Miller, Mark A. Chiu, J. Christine Min, Qilong Ogren, John A. TI An assessment of aerosol-cloud interactions in marine stratus clouds based on surface remote sensing SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID SATELLITE-DERIVED CLOUD; LARGE-EDDY SIMULATIONS; BOUNDARY-LAYER; ALBEDO; CLIMATE; POLLUTION; MICROPHYSICS; PARAMETERS; TRANSPORT; FRACTION AB An assessment of aerosol-cloud interactions (ACI) from ground-based remote sensing under coastal stratiform clouds is presented. The assessment utilizes a long-term, high temporal resolution data set from the Atmospheric Radiation Measurement (ARM) Program deployment at Pt. Reyes, California, United States, in 2005 to provide statistically robust measures of ACI and to characterize the variability of the measures based on variability in environmental conditions and observational approaches. The average ACI(N) (= dlnN(d)/dln alpha, the change in cloud drop number concentration with aerosol concentration) is 0.48, within a physically plausible range of 0-1.0. Values vary between 0.18 and 0.69 with dependence on (1) the assumption of constant cloud liquid water path (LWP), (2) the relative value of cloud LWP, (3) methods for retrieving N-d, (4) aerosol size distribution, (5) updraft velocity, and (6) the scale and resolution of observations. The sensitivity of the local, diurnally averaged radiative forcing to this variability in ACI(N) values, assuming an aerosol perturbation of 500 cm(-3) relative to a background concentration of 100 cm(-3), ranges between -4 and -9 W m(-2). Further characterization of ACI and its variability is required to reduce uncertainties in global radiative forcing estimates. C1 [McComiskey, Allison] Univ Colorado, Cooperat Inst Res Environm Sci, Boulder, CO 80309 USA. [McComiskey, Allison; Feingold, Graham; Frisch, A. Shelby] NOAA, Earth Syst Res Lab, Div Chem Sci, Boulder, CO 80305 USA. [Frisch, A. Shelby] Colorado State Univ, Cooperat Inst Res Atmosphere, Ft Collins, CO 80523 USA. [Turner, David D.] Univ Wisconsin, Ctr Space Sci & Engn, Madison, WI 53706 USA. [Miller, Mark A.] Rutgers State Univ, Dept Environm Sci, New Brunswick, NJ 08901 USA. [Chiu, J. Christine] Univ Maryland, Joint Ctr Earth Syst Technol, Baltimore, MD 21201 USA. [Chiu, J. Christine] NASA, Goddard Space Flight Ctr, Baltimore, MD USA. [Min, Qilong] SUNY Albany, Atmospher Sci Res Ctr, Albany, NY 12203 USA. [Ogren, John A.] NOAA, Earth Syst Res Lab, Global Monitoring Div, Boulder, CO 80305 USA. RP McComiskey, A (reprint author), Univ Colorado, Cooperat Inst Res Environm Sci, Boulder, CO 80309 USA. EM allison.mccomiskey@noaa.gov RI Feingold, Graham/B-6152-2009; Chiu, Christine/E-5649-2013; McComiskey, Allison/I-3933-2013; Ogren, John/M-8255-2015; Manager, CSD Publications/B-2789-2015 OI Chiu, Christine/0000-0002-8951-6913; McComiskey, Allison/0000-0002-6125-742X; Ogren, John/0000-0002-7895-9583; FU U.S. Department of Energy Office of Science [DE-AI02-06ER64215, DE-FG02-06ER64167, DE-FG0208ER64563, DE-FG02-03ER63531] FX This work was supported by the Atmospheric Radiation Measurement Program of the U.S. Department of Energy Office of Science under grants DE-AI02-06ER64215, DE-FG02-06ER64167, DE-FG0208ER64563, and DE-FG02-03ER63531. NR 55 TC 59 Z9 59 U1 1 U2 16 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 MAY 5 PY 2009 VL 114 AR D09203 DI 10.1029/2008JD011006 PG 15 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 443SB UT WOS:000265929800002 ER PT J AU Lee, HW You, W Barman, S Hellstrom, S LeMieux, MC Oh, JH Liu, S Fujiwara, T Wang, WM Chen, B Jin, YW Kim, JM Bao, ZA AF Lee, Hang Woo You, Wei Barman, Soumendra Hellstrom, Sondra LeMieux, Melburne C. Oh, Joon Hak Liu, Shuhong Fujiwara, Takenori Wang, Wechung Maria Chen, Bin Jin, Yong Wan Kim, Jong Min Bao, Zhenan TI Lyotropic Liquid-Crystalline Solutions of High-Concentration Dispersions of Single-Walled Carbon Nanotubes with Conjugated Polymers SO SMALL LA English DT Article DE alignment; carbon nanotubes; conjugated polymers; lyotropic liquid crystals ID THIN-FILM TRANSISTORS; OPTICAL-PROPERTIES; SEPARATION; SOLUBILIZATION; MORPHOLOGY; ALIGNMENT; NETWORKS; DEVICES; ARRAYS; WATER C1 [Lee, Hang Woo; You, Wei; Barman, Soumendra; Hellstrom, Sondra; LeMieux, Melburne C.; Oh, Joon Hak; Liu, Shuhong; Fujiwara, Takenori; Wang, Wechung Maria; Bao, Zhenan] Stanford Univ, Dept Chem Engn, Stanford, CA 94305 USA. [Chen, Bin] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Jin, Yong Wan; Kim, Jong Min] Samsung Adv Inst Technol, Younggin Si Gyunggi Do 449712, South Korea. RP Bao, ZA (reprint author), Stanford Univ, Dept Chem Engn, 381 North South Mall, Stanford, CA 94305 USA. EM zbao@stanford.edu RI Oh, Joon Hak/F-1454-2010; You, Wei/C-1333-2011; Liu, Sheng/K-2815-2013 OI Oh, Joon Hak/0000-0003-0481-6069; NR 38 TC 33 Z9 33 U1 2 U2 27 PU WILEY-V C H VERLAG GMBH PI WEINHEIM PA PO BOX 10 11 61, D-69451 WEINHEIM, GERMANY SN 1613-6810 J9 SMALL JI Small PD MAY 4 PY 2009 VL 5 IS 9 BP 1019 EP 1024 DI 10.1002/smll.200800640 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 447IJ UT WOS:000266184500004 PM 19291730 ER PT J AU Xie, H Li, YF Kagawa, HK Trent, JD Mudalige, K Cotlet, M Swanson, BI AF Xie, Hongzhi Li, Yi-Fen Kagawa, Hiromi K. Trent, Jonathan D. Mudalige, Kumara Cotlet, Mircea Swanson, Basil I. TI An Intrinsically Fluorescent Recognition Ligand Scaffold Based on Chaperonin Protein and Semiconductor Quantum-Dot Conjugates SO SMALL LA English DT Article DE nanoparticles; proteins; quantum dots; semiconductors ID HYPERTHERMOPHILIC ARCHAEON; NANOPARTICLE ARRAYS; SULFOLOBUS-SHIBATAE; AQUEOUS-SOLUTION; MOLECULES; NANOSTRUCTURES; EXCITATION; DYNAMICS; TF55 AB Genetic engineering of a novel protein-nanoparticle hybrid system with great potential for biosensing applications and for patterning of various types of nanoparticles is described. The hybrid system is based on a genetically modified chaperonin protein from the hyperthermophilic archaeon Sulfolobus shibatae. This chaperonin is an 18-subunit double ring, which self-assembles in the presence of Mg ions and ATP. Described here is a mutant chaperonin (His-beta-loopless, HBLL) with. increased access to the central cavity and His-tags on each subunit extending into the central cavity. This mutant binds water-soluble semiconductor quantum dots, creating a protein-encapsulated fluorescent nanoparticle. The new bioconjugate has high affinity, in the order of strong antibody-antigen interactions, a one-to-one protein-nanoparticle stoichiometry, and high stability. By adding selective binding sites to the solvent-exposed regions of the chaperonin, this protein-nanoparticle bioconjugate becomes a sensor for specific targets. C1 [Mudalige, Kumara; Cotlet, Mircea] Brookhaven Natl Lab, Ctr Funct Nanomat, Upton, NY 11973 USA. [Xie, Hongzhi; Swanson, Basil I.] Los Alamos Natl Lab, Div Chem, Los Alamos, NM 87545 USA. [Li, Yi-Fen; Kagawa, Hiromi K.; Trent, Jonathan D.] NASA, Ames Res Ctr, Bioengn Branch, Moffett Field, CA 94035 USA. RP Cotlet, M (reprint author), Brookhaven Natl Lab, Ctr Funct Nanomat, Mail Stop 735, Upton, NY 11973 USA. EM cotlet@bnl.gov; basil@lanl.gov RI Cotlet, Mircea/C-5004-2008 NR 32 TC 12 Z9 12 U1 0 U2 8 PU WILEY-V C H VERLAG GMBH PI WEINHEIM PA BOSCHSTRASSE 12, D-69469 WEINHEIM, GERMANY SN 1613-6810 J9 SMALL JI Small PD MAY 4 PY 2009 VL 5 IS 9 BP 1036 EP 1042 DI 10.1002/smll.200801106 PG 7 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 447IJ UT WOS:000266184500007 PM 19334012 ER PT J AU Roeser, HP Leschinski, P Huber, FM von Schoenermark, MF Nikoghosyan, AS Toberman, M AF Roeser, H. P. Leschinski, P. Huber, F. M. von Schoenermark, M. F. Nikoghosyan, A. S. Toberman, M. TI Oxygen deficiency structure in iron-based high temperature superconductor GdFeAsO1-delta SO ACTA ASTRONAUTICA LA English DT Article DE Iron-based high temperature superconductor; Superconducting unit area; Superconducting carrier density AB Oxygen deficiency in the iron-based HTSC GdFeAsO1-delta seems to create a parallelogram shaped Fe2+-ion/oxygen deficiency pattern in the Fe2O2 plane in c-direction. These two-dimensional nanostructures form Superconducting current channels which are separated by h = 0.828nm. The doping distance in direction of the super-current shows a strong correlation to the transition temperature. (C) 2008 Elsevier Ltd. All rights reserved. C1 [Roeser, H. P.; Leschinski, P.; von Schoenermark, M. F.] Univ Stuttgart, Inst Space Syst, D-70569 Stuttgart, Germany. [Huber, F. M.] Steinbeis Transferzentrum Raumfahrt, D-71126 Gaeufelden, Germany. [Nikoghosyan, A. S.] Yerevan State Univ, Dept Microwave & Telecommun, Yerevan 375025, Armenia. [Toberman, M.] NASA, Dryden Flight Res Ctr, Edwards AFB, CA 93523 USA. RP Roeser, HP (reprint author), Univ Stuttgart, Inst Space Syst, Pfaffenwaldring 31, D-70569 Stuttgart, Germany. EM roeser@irs.uni-stuttgart.de NR 7 TC 1 Z9 1 U1 0 U2 1 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0094-5765 J9 ACTA ASTRONAUT JI Acta Astronaut. PD MAY-JUN PY 2009 VL 64 IS 9-10 BP 1011 EP 1013 DI 10.1016/j.actaastro.2008.11.010 PG 3 WC Engineering, Aerospace SC Engineering GA 432QB UT WOS:000265148100016 ER PT J AU Mertens, CJ Winick, JR Picard, RH Evans, DS Lopez-Puertas, M Wintersteiner, PP Xu, XJ Mlynczak, MG Russell, JM AF Mertens, Christopher J. Winick, Jeremy R. Picard, Richard H. Evans, David S. Lopez-Puertas, Manuel Wintersteiner, Peter P. Xu, Xiaojing Mlynczak, Martin G. Russell, James M., III TI Influence of solar-geomagnetic disturbances on SABER measurements of 4.3 mu m emission and the retrieval of kinetic temperature and carbon dioxide SO ADVANCES IN SPACE RESEARCH LA English DT Article DE SABER; Temperature; Carbon Dioxide (CO2); Infrared remote sensing; Non-LTE; Radiation Transfer; Ionosphere E-Region; Magnetic Storms; E-Region Ion-Neutral Chemistry ID RADIATIVE-TRANSFER MODEL; ROTATIONALLY EXCITED NO+; ION-MOLECULE REACTION; MIDDLE ATMOSPHERE; AURORAL ELECTRONS; UPPER MESOSPHERE; INFRARED BANDS; LIMB EMISSION; GROUND-STATE; CO2 AB Thermospheric infrared radiance at 4.3 mu m is susceptible to the influence of solar-geomagnetic disturbances. Ionization processes followed by ion-neutral chemical reactions lead to vibrationally excited NO+ (i.e., NO+(v)) and subsequent 4.3 mu m emission in the ionospheric E-region. Large enhancements of nighttime 4.3 mu m emission were observed by the TIMED/SABER instrument during the April 2002 and October-November 2003 solar storms. Global measurements of infrared 4.3 mu m emission provide an excellent proxy to observe the nighttime E-region response to auroral dosing and to conduct a detailed study of E-region ion-neutral chemistry and energy transfer mechanisms. Furthermore, we find that photoionization processes followed by ion-neutral reactions during quiescent. daytime conditions increase the NW concentration enough to introduce biases in the TIMED/SABER operational processing of kinetic temperature and CO2 data, with the largest effect at summer solstice. In this paper. we discuss solar storm enhancements of 4.3 mu m emission observed from SABER and assess the impact of NO+ (v) 4.3 mu m emission on quiescent. daytime retrievals of Tk/CO2 from the SABER instrument. Published by Elsevier Ltd. on behalf of COSPAR C1 [Mertens, Christopher J.] NASA, Langley Res Ctr, Hampton, VA 23681 USA. [Winick, Jeremy R.; Picard, Richard H.] USAF, Res Lab, Hanscom AFB, MA 01731 USA. [Evans, David S.] NOAA, Space Weather Predict Ctr, Boulder, CO 80303 USA. [Lopez-Puertas, Manuel] CSIC, Inst Astrofis Andalucia, E-18080 Granada, Spain. [Wintersteiner, Peter P.] ARCON Corp, Waltham, MA 02451 USA. [Xu, Xiaojing] SSAI Inc, Hampton, VA 23666 USA. [Mlynczak, Martin G.] NASA, Langley Res Ctr, Hampton, VA 23681 USA. [Russell, James M., III] Hampton Univ, Hampton, VA 23668 USA. RP Mertens, CJ (reprint author), NASA, Langley Res Ctr, 21 Langley Blvd,MS 401B, Hampton, VA 23681 USA. EM Christopher.J.Mertens@nasa.gov; jeremy.winick@hanscom.af.mil; richard.picard@hanscom.af.mil; David.S.Evans@noaa.gov; puertas@iaa.es; winters@arcon.com; xiaojing_xu@ssaihq.com; Martin.G.Mlynczak@nasa.gov; james.russell@hamptonu.edu RI Mlynczak, Martin/K-3396-2012; Lopez Puertas, Manuel/M-8219-2013 OI Lopez Puertas, Manuel/0000-0003-2941-7734 NR 51 TC 9 Z9 9 U1 0 U2 1 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 0273-1177 EI 1879-1948 J9 ADV SPACE RES JI Adv. Space Res. PD MAY 1 PY 2009 VL 43 IS 9 BP 1325 EP 1336 DI 10.1016/j.asr.2008.10.029 PG 12 WC Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences GA 442DV UT WOS:000265821100003 ER PT J AU Liou, JC Johnson, NL AF Liou, J. -C. Johnson, N. L. TI Characterization of the cataloged Fengyun-1C fragments and their long-term effect on the LEO environment SO ADVANCES IN SPACE RESEARCH LA English DT Article DE Orbital debris; Environment; Modeling; Fengyun1-C ID MODEL AB The intentional breakup of Fengyun-1C on I I January 2007 created the most severe orbital debris cloud in history. The altitude where the event Occurred was probably the worst location for a major breakup ill the low Earth orbit (LEO) region, since it was already highly populated with operational satellites and debt-is generated from previous breakups. The addition of so many fragments not only poses a realistic threat to operational satellites in the region, but also increases the instability (i.e., collision cascade effect) of the debris population there. Detailed analysis of the large Fengyun-1C fragments indicates that their size and area-to-mass ratio (A/M) distributions are very different from those of other known events. About half of the fragments appear to be composed of light-weight materials and more than 100 of them have A/M values exceeding 1 m(2)/kg, consistent with thermal blanket and solar panel pieces. In addition, the orbital elements of the fragments suggest non-trivial velocity gain by the fragment cloud during the impact. These important characteristics were incorporated into numerical simulations to assess the long-term impact of the Fengyun-1C fragments to the LEO debris environment. The collision probabilities between the Fengyun-1C fragments and the rest of the catalog Population and the population growth in the low Earth orbit region in the next 100 years are summarized in the paper, Published by Elsevier Ltd. on behalf of COSPAR. C1 [Liou, J. -C.; Johnson, N. L.] NASA, Orbital Debris Program Off, Johnson Space Ctr, Houston, TX 77058 USA. RP Liou, JC (reprint author), NASA, Orbital Debris Program Off, Johnson Space Ctr, 2101 NASA Pkwy, Houston, TX 77058 USA. EM jer-chyi.liou-l@nasa.gov NR 6 TC 11 Z9 11 U1 0 U2 3 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 0273-1177 J9 ADV SPACE RES JI Adv. Space Res. PD MAY 1 PY 2009 VL 43 IS 9 BP 1407 EP 1415 DI 10.1016/j.asr.2009.01.011 PG 9 WC Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences GA 442DV UT WOS:000265821100011 ER PT J AU Balakumar, P AF Balakumar, P. TI Receptivity of a Supersonic Boundary Layer to Acoustic Disturbances SO AIAA JOURNAL LA English DT Article; Proceedings Paper CT AIAA 43rd Aerospace Sciences Meeting and Exhibit CY JAN 10-13, 2005 CL Reno, NV SP AIAA ID LEADING-EDGE RECEPTIVITY; FLAT-PLATE; TRANSITION; STABILITY AB The boundary layer receptivity process generated by the interaction of 3-D slow and fast acoustic disturbances with a blunted flat plate, is numerically investigated at a freestream Mach number of 3.5, and at a high Reynolds number of 39 * 10(6)/m. The computations are performed with and without a 2-D isolated roughness element located near the leading edge. Both the steady and unsteady solutions are obtained by solving the full Navier-Stokes equations using the fifth-order accurate weighted essentially nonoscillatory scheme for space discretization and using the third-order total-variation-diminishing Runge-Kutta scheme for time integration. The simulations showed that the linear instability waves are generated very close to the leading edge. The wavelength of the disturbances inside the boundary layer first increases gradually and becomes longer than the wavelength for the instability waves within a short distance from the leading edge. The wavelength then decreases gradually and merges with the wavelength for the Tollmien-Schlichting wave. The initial amplitudes of the instability waves near the neutral points, the receptivity coefficients, are about 1.20 and 0.07 times the amplitude of the freestream disturbances for the slow and fast waves, respectively. It was also revealed that a small isolated roughness element does not enhance the receptivity process for the given nose bluntness. C1 NASA, Langley Res Ctr, Flow Phys & Control Branch, Hampton, VA 23681 USA. RP Balakumar, P (reprint author), NASA, Langley Res Ctr, Flow Phys & Control Branch, Mail Stop 170, Hampton, VA 23681 USA. NR 19 TC 11 Z9 11 U1 1 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 MAY PY 2009 VL 47 IS 5 BP 1069 EP 1078 DI 10.2514/1.33395 PG 10 WC Engineering, Aerospace SC Engineering GA 438WH UT WOS:000265586200002 ER PT J AU Mascarenhas, BS Helenbrook, BT Atkins, HL AF Mascarenhas, Brendan S. Helenbrook, Brian T. Atkins, Harold L. TI Application of p-Multigrid to Discontinuous Galerkin Formulations of the Euler Equations SO AIAA JOURNAL LA English DT Article; Proceedings Paper CT AIAA 18th Computational Fluid Dynamics Conference CY JUN 25-28, 2007 CL Miami, FL SP Amer Inst Aeronaut & Astronaut ID NAVIER-STOKES EQUATIONS; FLOWS AB We have investigated the p-multigrid iterative method for solving p = 1, 2, and 4 discontinuous Galerkin approximations to the Enter equations where p is the degree of the approximating polynomial. For comparison, we have also investigated agglomeration multigrid for p = 0 approximations. Block diagonal, line, and sweeping relaxation schemes were examined. The convergence rate to a uniform flow on a structured mesh was analyzed as a function of the flow angle relative to the mesh, grid resolution, underrelaxation factor used, and Mach number. The result,; show that, even for this simplified problem, many of these schemes do not perform well. For p = 0, which corresponds to a conventional finite volume discretization, only the block symmetric Gauss-Seidel line relaxation and the Gauss-Seidel alternate direction line relaxation performed well under all conditions. For p > 0, all schemes converged slower than the corresponding p = 0 case. Furthermore, all of the schemes were more sensitive to flow angle and Mach number than with p = 0. We also found that two-level p-multigrid performs anomalously for p = I to 0. This behavior is illustrated and explained. C1 [Mascarenhas, Brendan S.; Helenbrook, Brian T.] Clarkson Univ, Dept Mech & Aeronaut Engn, Potsdam, NY 13699 USA. [Atkins, Harold L.] NASA, Langley Res Ctr, Computat AcroSci Branch, Hampton, VA 23681 USA. RP Mascarenhas, BS (reprint author), Clarkson Univ, Dept Mech & Aeronaut Engn, Potsdam, NY 13699 USA. EM mascarbs@clarkson.edu; helenbrk@clarkson.edu; harold.l.atkins@nasa.gov NR 18 TC 6 Z9 6 U1 0 U2 1 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 MAY PY 2009 VL 47 IS 5 BP 1200 EP 1208 DI 10.2514/1.39765 PG 9 WC Engineering, Aerospace SC Engineering GA 438WH UT WOS:000265586200014 ER PT J AU Mikouchi, T Zolensky, M Ivanova, M Tachikawa, O Komatsu, M Le, L Gounelle, M AF Mikouchi, Takashi Zolensky, Michael Ivanova, Marina Tachikawa, Osamu Komatsu, Mutsumi Le, Loan Gounelle, Matthieu TI Dmitryivanovite: A new high-pressure calcium aluminum oxide from the Northwest Africa 470 CH3 chondrite characterized using electron backscatter diffraction analysis SO AMERICAN MINERALOGIST LA English DT Article DE Dmitryivanovite; CAI; electron backscatter diffraction; new minerals; CH chondrite ID CARBONACEOUS CHONDRITE; GROSSITE CAAL4O7; RICH INCLUSIONS; METAL GRAINS; CONDENSATION; PATTERNS; PHASE; IDENTIFICATION; MONOALUMINATE; MICROSCOPE AB Dmitryivanovite (CaAl(2)O(4)) is a newly described, calcium aluminium oxide from the Northwest Africal 470 (NWA470) CH3 chondrite (Ivanova et al. 2002). NWA470 contains abundant small Ca,Al-rich inclusions (CAIs), and dmitryivanovite, whose composition is close to stoichiometric CaAl(2)O(4) [Ca(1.000)(Al(1.993)Si(0.003)Ti(0.002))(1.992)O(4)], was found in one of these CAIs. It occurs as similar to 10 mu m subhedral grains intergrown with grossite (CaAl(4)O(7)), perovskite, and melilite. Electron backscatter diffraction (EBSD) analysis revealed that dmitryivanovite is a high-pressure polymorph of CaAl(2)O(4) (a = 7.95, b = 8.68, c = 10.25 angstrom, beta = 9.31 degrees, space group P2(1)/c, and Z = 12). Dmitryivanovite is the third phase to be described from nature in the binary system of CaO-Al(2)O(3), the other two being hibonite (CaAl(12)O(19)) and grossite (CaAl(4)O(7))-all are found in CAIs. The presence of CaAl(2)O(4) in NWA470 suggests a local elevated dust/gas ratio in the solar nebula. The phase diagram of CaAl(2)O(4) shows that similar to 2 GPa is required to stabilize the high-pressure CaAl(2)O(4) polymorph at 1327 degrees C, above which CaAl(2)O(4) condenses from the solar nebula. Because it is unlikely that the solar nebula ever had such a high total gas pressure, it appears more probable that condensation of the low-pressure polymorph occurred in the solar nebula with an enhanced dust-to-gas ratio and that subsequently the high-pressure polymorph was produced by shock metamorphism, most liekly after the CaAl(2)O(4)-bearing CAI was incorporated into the NWA470 parent asteroid. C1 [Mikouchi, Takashi; Tachikawa, Osamu; Komatsu, Mutsumi] Univ Tokyo, Grad Sch Sci, Dept Earth & Planetary Sci, Bunkyo Ku, Tokyo 1130033, Japan. [Zolensky, Michael] NASA, Lyndon B Johnson Space Ctr, Code KT, Houston, TX 77058 USA. [Ivanova, Marina] Vernadsky Inst Geochem, Moscow 119991, Russia. [Le, Loan] Jacobs Sverdrup Co, Houston, TX 77058 USA. [Gounelle, Matthieu] Museum Natl Hist Nat, Lab Etud Mat Extraterrestre, F-75005 Paris, France. RP Mikouchi, T (reprint author), Univ Tokyo, Grad Sch Sci, Dept Earth & Planetary Sci, Bunkyo Ku, Tokyo 1130033, Japan. EM mikouchi@eps.s.u-tokyo.ac.jp FU Meteorite Committee; Russian Academy of Sciences; NASA FX We thank the Meteorite Committee, Russian Academy of Sciences, for the loan of a polished thin section of NWA470. We also thank K. Sugiyama for drawing the crystal structure of dmitryivanovite. A review of an earlier version of this manuscript by S. Simon and K. Lodders resulted in significant improvements, We thank R. Jones. D. Ebel. and A. Bischoff for their constructive reviews. R. Down kindly provided a copy of his XPow program. This work was supported in part by NASA Cosmochemistry Program and Hayabusa Program grants to M. Zolensky, Electron microscopy was performed in the Electron Microbeam Analysis Facility for Mineralogy in the Department of Earth and Planetary Science, University of Tokyo. NR 33 TC 8 Z9 8 U1 1 U2 11 PU MINERALOGICAL SOC AMER PI CHANTILLY PA 3635 CONCORDE PKWY STE 500, CHANTILLY, VA 20151-1125 USA SN 0003-004X J9 AM MINERAL JI Am. Miner. PD MAY-JUN PY 2009 VL 94 IS 5-6 BP 746 EP 750 DI 10.2138/am.2009.3080 PG 5 WC Geochemistry & Geophysics; Mineralogy SC Geochemistry & Geophysics; Mineralogy GA 445VA UT WOS:000266078400011 ER PT J AU Casner, SM AF Casner, Stephen M. TI Perceived vs. measured effects of advanced cockpit systems on pilot workload and error: Are pilots' beliefs misaligned with reality? SO APPLIED ERGONOMICS LA English DT Article DE Workload; Automation; Advanced cockpit systems; Error AB Four types of advanced cockpit systems were tested in an in-flight experiment for their effect on pilot workload and error. Twelve experienced pilots flew conventional cockpit and advanced cockpit versions of the same make and model airplane. in both airplanes, the experimenter dictated selected combinations of cockpit systems for each pilot to use while soliciting subjective workload measures and recording any errors that pilots made. The results indicate that the use of a GPS navigation computer helped reduce workload and errors during some phases of flight but raised them in others. Autopilots helped reduce some aspects of workload in the advanced cockpit airplane but did not appear to reduce workload in the conventional cockpit. Electronic flight and navigation instruments appeared to have no effect on workload or error. Despite this modest showing for advanced cockpit systems, pilots stated an overwhelming preference for using them during all phases of flight. Published by Elsevier Ltd. C1 NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Casner, SM (reprint author), NASA, Ames Res Ctr, Mail Stop 262-4, Moffett Field, CA 94035 USA. EM casner@gmail.com NR 10 TC 9 Z9 9 U1 3 U2 7 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 0003-6870 J9 APPL ERGON JI Appl. Ergon. PD MAY PY 2009 VL 40 IS 3 BP 448 EP 456 DI 10.1016/j.apergo.2008.10.002 PG 9 WC Engineering, Industrial; Ergonomics; Psychology, Applied SC Engineering; Psychology GA 422UT UT WOS:000264453900018 PM 19028379 ER PT J AU Mishchenko, MI Liu, L AF Mishchenko, Michael I. Liu, Li TI Electromagnetic scattering by densely packed particulate ice at radar wavelengths: exact theoretical results and remote-sensing implications SO APPLIED OPTICS LA English DT Article ID COHERENT BACKSCATTERING; LIGHT-SCATTERING; SATURNS RINGS; PARTICLES; SPHERES; MODEL AB We use the numerically exact superposition T-matrix method to compute electromagnetic scattering characteristics of a macroscopic volume of a discrete random medium filled with wavelength-sized spherical particles with a refractive index typical of water ice at centimeter wavelengths. Our analysis demonstrates relative strengths of various optical observables in terms of their potential remote-sensing content. In particular, it illustrates the importance of accounting for the forward-scattering interference effect in the interpretation of occultation measurements of planetary rings. We show that among the most robust indicators of the amount of multiple scattering inside a particulate medium are the cross-polarized scattered intensity, the same-helicity scattered intensity, and the circular polarization ratio. We also demonstrate that many predictions of the low-packing-density theories of radiative transfer and coherent backscattering are applicable, both qualitatively and semi-quantitatively, to densely packed media. C1 [Mishchenko, Michael I.; Liu, Li] NASA, Goddard Inst Space Studies, New York, NY 10025 USA. [Liu, Li] Columbia Univ, New York, NY 10025 USA. RP Mishchenko, MI (reprint author), NASA, Goddard Inst Space Studies, 2880 Broadway, New York, NY 10025 USA. EM mmishchenko@giss.nasa.gov RI Mishchenko, Michael/D-4426-2012 FU NASA Radiation Sciences Program FX We are grateful to Joop Hovenier, Daniel Mackowski, Victor Tishkovets, Gorden Videen, and two anonymous reviewers for valuable comments and suggestions. This research was funded by the NASA Radiation Sciences Program managed by Hal Maring. NR 31 TC 16 Z9 16 U1 1 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 MAY 1 PY 2009 VL 48 IS 13 BP 2421 EP 2426 DI 10.1364/AO.48.002421 PG 6 WC Optics SC Optics GA 448JX UT WOS:000266260000002 PM 19412198 ER PT J AU Potter, EG Bebout, BM Kelley, CA AF Potter, Elyn G. Bebout, Brad M. Kelley, Cheryl A. TI Isotopic Composition of Methane and Inferred Methanogenic Substrates Along a Salinity Gradient in a Hypersaline Microbial Mat System SO ASTROBIOLOGY LA English DT Article DE Hypersaline microbial mats; Methane stable isotopes; Apparent fractionation factors; Methanogenic pathways ID METHYLATED AMINES; GUERRERO-NEGRO; CH4 OXIDATION; CARBON; PATHWAYS; FRACTIONATION; ECOSYSTEMS; DIVERSITY; MARS; LAKE AB The importance of hypersaline environments over geological time, the discovery of similar habitats on Mars, and the importance of methane as a biosignature gas combine to compel an understanding of the factors important in controlling methane released from hypersaline microbial mat environments. To further this understanding, changes in stable carbon isotopes of methane and possible methanogenic substrates in microbial mat communities were investigated as a function of salinity here on Earth. Microbial mats were sampled from four different field sites located within salterns in Baja California Sur, Mexico. Salinities ranged from 50 to 106 parts per thousand (ppt). Pore water and microbial mat samples were analyzed for the carbon isotopic composition of dissolved methane, dissolved inorganic carbon (DIC), and mat material (particulate organic carbon or POC). The POC delta(13)C values ranged from -6.7 to -13.5 parts per thousand, and DIC delta(13)C values ranged from -1.4 to -9.6 parts per thousand. These values were similar to previously reported values. The delta(13)C values of methane ranged from -49.6 to -74.1 parts per thousand; the methane most enriched in 13 C was obtained from the highest salinity area. The apparent fractionation factors between methane and DIC, and between methane and POC, within the mats were also determined and were found to change with salinity. The apparent fractionation factors ranged from 1.042 to 1.077 when calculated using DIC and from 1.038 to 1.068 when calculated using POC. The highest-salinity area showed the least fractionation, the moderate-salinity area showed the highest fractionation, and the lower-salinity sites showed fractionations that were intermediate. These differences in fractionation are most likely due to changes in the dominant methanogenic pathways and substrates used at the different sites because of salinity differences. C1 [Potter, Elyn G.; Kelley, Cheryl A.] Univ Missouri, Dept Geol Sci, Columbia, MO 65211 USA. [Bebout, Brad M.] NASA, Ames Res Ctr, Exobiol Branch, Moffett Field, CA 94035 USA. RP Kelley, CA (reprint author), Univ Missouri, Dept Geol Sci, 101 Geol Sci Bldg, Columbia, MO 65211 USA. EM kelleyc@missouri.edu RI Kelley, Cheryl/K-9392-2015 NR 45 TC 13 Z9 13 U1 0 U2 9 PU MARY ANN LIEBERT INC PI NEW ROCHELLE PA 140 HUGUENOT STREET, 3RD FL, NEW ROCHELLE, NY 10801 USA SN 1531-1074 J9 ASTROBIOLOGY JI Astrobiology PD MAY PY 2009 VL 9 IS 4 BP 383 EP 390 DI 10.1089/ast.2008.0260 PG 8 WC Astronomy & Astrophysics; Biology; Geosciences, Multidisciplinary SC Astronomy & Astrophysics; Life Sciences & Biomedicine - Other Topics; Geology GA 457GD UT WOS:000266915600005 PM 19400733 ER PT J AU Lindgren, P Parnell, J Bowden, S Taylor, C Osinski, GR Lee, P AF Lindgren, Paula Parnell, John Bowden, Stephen Taylor, Colin Osinski, Gordon R. Lee, Pascal TI Preservation of Biological Markers in Clasts Within Impact Melt Breccias from the Haughton Impact Structure, Devon Island SO ASTROBIOLOGY LA English DT Article DE Biomarkers; Impacts; Haughton Crater ID HYDROTHERMAL SYSTEMS; MATURITY PARAMETERS; MOLECULAR FOSSILS; MARTIAN LIFE; CRATER; MARS; RADIATION; CANADA; ROCKS AB The 39 +/- 2Ma Haughton impact structure on Devon Island comprises a thick target succession of sedimentary rocks, mainly carbonates. The carbonates contain pre-impact organic matter, including fossil biological markers. Haughton is located in an area where no major thermal event has affected the sedimentary succession after heating caused by impact. This makes Haughton uniquely suitable for studies concerning the preservation of fossil biological markers following an impact event. Melt breccia is the most common impactite at Haughton. It is composed of clasts of the target, mainly carbonates, embedded in a fine groundmass. The groundmass is composed of material that was melted during impact. In this study, fossil biological marker maturity parameters (tricyclic terpane-hopane ratio and pregnane-sterane ratio) and an aromatic maturity parameter [methylphenanthrene ratio (MPR)] were used to compare the degree of thermal alteration in different size fractions of carbonate clasts (<0.5-4 cm in diameter) and between edges and centers of large carbonate clasts (15-20 cm in diameter). The data show that fossil biological markers can be preserved and detected in isolated large and small fractions of carbonate clasts that are embedded in an impact melt. The results also indicate that there is a thermal gradient from the center of a clast to the edge of a clast, which suggests that biological markers are more likely to be found preserved in the center of a clast. The thermal maturity values point to a higher degree of thermal alteration in the melt breccia carbonate clasts than in the coherent carbonate bedrock. C1 [Lindgren, Paula] Stockholm Univ, Dept Geol & Geochem, S-10691 Stockholm, Sweden. [Lindgren, Paula; Parnell, John; Bowden, Stephen; Taylor, Colin] Univ Aberdeen, Dept Geol & Petr Geol, Aberdeen, Scotland. [Osinski, Gordon R.] Univ Western Ontario, Dept Earth Sci, London, ON, Canada. [Osinski, Gordon R.] Univ Western Ontario, Dept Phys & Astron, London, ON, Canada. [Lee, Pascal] NASA, Ames Res Ctr, SETI, Moffett Field, CA 94035 USA. RP Lindgren, P (reprint author), Stockholm Univ, Dept Geol & Geochem, S-10691 Stockholm, Sweden. EM paula.lindgren@geo.su.se NR 27 TC 3 Z9 3 U1 1 U2 4 PU MARY ANN LIEBERT INC PI NEW ROCHELLE PA 140 HUGUENOT STREET, 3RD FL, NEW ROCHELLE, NY 10801 USA SN 1531-1074 J9 ASTROBIOLOGY JI Astrobiology PD MAY PY 2009 VL 9 IS 4 BP 391 EP 400 DI 10.1089/ast.2008.0270 PG 10 WC Astronomy & Astrophysics; Biology; Geosciences, Multidisciplinary SC Astronomy & Astrophysics; Life Sciences & Biomedicine - Other Topics; Geology GA 457GD UT WOS:000266915600006 PM 19519214 ER PT J AU Jacobson, RA AF Jacobson, R. A. TI THE ORBITS OF THE NEPTUNIAN SATELLITES AND THE ORIENTATION OF THE POLE OF NEPTUNE SO ASTRONOMICAL JOURNAL LA English DT Article DE ephemerides; planets and satellites: individual (Neptune, Nereid, Proteus, Triton) ID OUTER PLANETS; ASTROMETRIC OBSERVATIONS; FASTT OBSERVATIONS; CCD OBSERVATIONS; POSITIONS; NEREID; TRITON; PROTEUS; VOYAGER AB This paper reports on an update to the orientation of Neptune's pole and to the orbits of the Neptunian satellites, Triton, Nereid, and Proteus. We determined the new pole and orbits in the International Celestial Reference Frame by fitting them to all available observations through the opposition of 2008. The new data in the fit are high-quality modern astrometry and constitute a 19 year extension of the previous data arc. We assess the accuracy of the orbits and compare them with our earlier orbits. We also provide mean elements as a geometrical description for the orbits. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Jacobson, RA (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM robert.jacobson@jpl.nasa.gov FU National Aeronautics and Space Administration FX The research described in this publication was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. NR 44 TC 34 Z9 34 U1 0 U2 5 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 MAY PY 2009 VL 137 IS 5 BP 4322 EP 4329 DI 10.1088/0004-6256/137/5/4322 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 430WB UT WOS:000265019900016 ER PT J AU Duran-Rojas, MC Watson, AM Stapelfeldt, KR Hiriart, D AF Carolina Duran-Rojas, Maria Watson, Alan M. Stapelfeldt, Karl R. Hiriart, David TI THE POLARIMETRIC AND PHOTOMETRIC VARIABILITY OF HH 30 SO ASTRONOMICAL JOURNAL LA English DT Article DE accretion, accretion disks; circumstellar matter; stars: individual (HH 30); stars: pre-main sequence ID T-TAURI STARS; SPACE-TELESCOPE OBSERVATIONS; ORION NEBULA CLUSTER; HERBIG-HARO OBJECTS; PHOTOPOLARIMETRIC VARIABILITY; CIRCUMSTELLAR DISK; LINEAR-POLARIZATION; MAGNETIC ACCRETION; AA-TAU; HH-30 AB We have obtained ground-based photopolarimetry of the young stellar object HH 30 over the course of one year. Our observations reveal the presence of a dominant periodic modulation of the polarization with a period of 7.49 +/- 0.04 days or one of the aliases of this period close to 1 day. There are also suggestions of a weak periodic modulation in the photometry with the same period but a phase displaced by one quarter of a period. These results are in agreement with the lighthouse model for HH 30, in which a beam or shadow from a central source sweeps across the disk. Our observations by themselves appear to be consistent with both of the mechanisms that have been proposed for the lighthouse-asymmetric accretion hot spots on the star or orbiting clumps or voids in the disk-and provide strong quantitative constraints for future models. C1 [Carolina Duran-Rojas, Maria; Watson, Alan M.] Univ Nacl Autonoma Mexico, Ctr Radioastron & Astrofis, Morelia 58089, Michoacan, Mexico. [Watson, Alan M.] Univ Nacl Autonoma Mexico, Inst Astron, Mexico City 04510, DF, Mexico. [Stapelfeldt, Karl R.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Hiriart, David] Univ Nacl Autonoma Mexico, Inst Astron, Ensenada 22800, Baja California, Mexico. RP Duran-Rojas, MC (reprint author), Univ Nacl Autonoma Mexico, Ctr Radioastron & Astrofis, Apartado Postal 3-72 Xangari, Morelia 58089, Michoacan, Mexico. EM c.duran@astrosmo.unam.mx; alan@astrosc.unam.mx; krs@exoplanet.jpl.nasa.gov; hiriart@astrosen.unam.mx RI Stapelfeldt, Karl/D-2721-2012 FU National Aeronautics and Space Administration; National Science Foundation FX We thank Kenny Wood for suggesting that we monitor the polarization of HH 30. We also thank an anonymous referee for a useful report. We are extremely grateful to the staff of the OAN/SPM for their support and warm hospitality during several long observing runs. We thank Jorge Valdez, Fernando Quiros, Benjamin Garcia, and Esteban Luna for their contributions to the design and construction of POLIMA. M. C. D. R. thanks CONACyT for a graduate student fellowship. K. R. S. acknowledges funding support to the Spitzer Space Telescope Project Science Office. We used the IRAF software for some data reduction. IRAF is distributed by the National Optical Astronomy Observatories, which is operated by the Association of Universities for Research in Astronomy, Inc., under cooperative agreement with the National Science Foundation. We also used data products from the Two Micron All Sky Survey, which is a joint project of the University of Massachusetts and the Infrared Processing and Analysis Center at the California Institute of Technology, funded by the National Aeronautics and Space Administration and the National Science Foundation. NR 34 TC 5 Z9 5 U1 0 U2 2 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 MAY PY 2009 VL 137 IS 5 BP 4330 EP 4338 DI 10.1088/0004-6256/137/5/4330 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 430WB UT WOS:000265019900017 ER PT J AU Miller, NA Hornschemeier, AE Mobasher, B AF Miller, Neal A. Hornschemeier, Ann E. Mobasher, Bahram TI A DEEP VERY LARGE ARRAY RADIO CONTINUUM SURVEY OF THE CORE AND OUTSKIRTS OF THE COMA CLUSTER SO ASTRONOMICAL JOURNAL LA English DT Article DE galaxies: clusters: general; galaxies: clusters: individual (Abell 1656); radio continuum: galaxies ID DIGITAL SKY SURVEY; EARLY-TYPE GALAXIES; BRIGHTEST SPIRAL GALAXIES; GIANT GALAXIES; LUMINOSITY FUNCTION; NEARBY CLUSTERS; DATA RELEASE; ELLIPTIC GALAXIES; SOURCE POPULATION; HUBBLE CONSTANT AB We present deep 1.4 GHz Very Large Array radio continuum observations of two similar to 0.5 deg(2) fields in the Coma cluster of galaxies. The two fields, "Coma 1" and "Coma 3," correspond to the cluster core and southwest infall region and were selected on account of abundant preexisting multiwavelength data. In their most sensitive regions the radio data reach 22 mu Jy rms per 4 ''.4 beam, sufficient to detect (at 5 sigma) Coma member galaxies with L(1.4GHz) = 1.3 x 10(20) W Hz(-1). The full catalog of radio detections is presented herein and consists of 1030 sources detected at >= 5 sigma, 628 of which are within the combined Coma 1 and Coma 3 area. We also provide optical identifications of the radio sources using data from the Sloan Digital Sky Survey. The depth of the radio observations allows us to detect active galactic nucleus in cluster elliptical galaxies with M(r) < -20.5 (AB magnitudes), including radio detections for all cluster ellipticals with M(r) < -21.8. At fainter optical magnitudes (-20.5 < M(r) greater than or similar to -19), the radio sources are associated with star-forming galaxies with star formation rates as low as 0.1 M(circle dot) yr(-1). C1 [Miller, Neal A.; Hornschemeier, Ann E.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Hornschemeier, Ann E.] NASA, Goddard Space Flight Ctr, Lab Xray Astrophys, Greenbelt, MD 20771 USA. [Mobasher, Bahram] Univ Calif Riverside, Dept Phys & Astron, Riverside, CA 92521 USA. RP Miller, NA (reprint author), Johns Hopkins Univ, Dept Phys & Astron, 3400 N Charles St, Baltimore, MD 21218 USA. EM nmiller@pha.jhu.edu FU National Aeronautics and Space Administration FX This research has made use of the NED which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. NR 61 TC 9 Z9 9 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 MAY PY 2009 VL 137 IS 5 BP 4436 EP 4449 DI 10.1088/0004-6256/137/5/4436 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 430WB UT WOS:000265019900025 ER PT J AU Miller, NA Hornschemeier, AE Mobasher, B Bridges, TJ Hudson, MJ Marzke, RO Smith, RJ AF Miller, Neal A. Hornschemeier, Ann E. Mobasher, Bahram Bridges, Terry J. Hudson, Michael J. Marzke, Ronald O. Smith, Russell J. TI THE RADIO LUMINOSITY FUNCTION AND GALAXY EVOLUTION IN THE COMA CLUSTER SO ASTRONOMICAL JOURNAL LA English DT Article DE galaxies: clusters: individual (Abell 1656); galaxies: evolution; galaxies: luminosity function, mass function; radio continuum: galaxies ID DIGITAL SKY SURVEY; MORPHOLOGY-DENSITY RELATION; STAR-FORMATION HISTORIES; COLOR-MAGNITUDE DIAGRAM; ACTIVE GALACTIC NUCLEI; LOCAL UNIVERSE; DISTANT CLUSTERS; GIANT GALAXIES; ABELL CLUSTERS; RICH CLUSTERS AB We investigate the radio luminosity function and radio source population for two fields within the Coma cluster of galaxies, with the fields centered on the cluster core and southwest infall region and each covering about half a square degree. Using VLA data with a typical rms sensitivity of 28 mu Jy per 4 ''.4 beam, we identify 249 radio sources with optical counterparts brighter than r = 22. For cluster galaxies, these correspond to L(1.4) = 1.7 x 10(20) W Hz(-1)(for a 5 sigma source) and M(r) = -13. Comprehensive optical spectroscopy identifies 38 of these as members of the Coma cluster, evenly split between sources powered by an active nucleus and sources powered by active star formation. The radio-detected star-forming galaxies are the dominant population only at radio luminosities between about 10(21) and 10(22) WHz(-1), an interesting result given star formation dominates field radio luminosity functions for all luminosities lower than about 10(23) W Hz(-1). The majority of the radio-detected star-forming galaxies have characteristics of starbursts, including high specific star formation rates and optical spectra with strong emission lines. In conjunction with prior studies on post-starburst galaxies within the Coma cluster, this is consistent with a picture in which late-type galaxies entering Coma undergo a starburst prior to a rapid cessation of star formation. Optically bright elliptical galaxies (M(r) <= -20.5) make the largest contribution to the radio luminosity function at both the high (greater than or similar to 3 x 10(22) WHz(-1)) and low (less than or similar to 10(21) WHz(-1)) ends. Through a stacking analysis of these optically bright ellipticals we find that they continue to harbor radio sources down to luminosities as faint as 3 x 10(19) W Hz(-1). However, contrary to published results for the Virgo cluster we find no evidence for the existence of a population of optically faint (M(r) approximate to -14) dwarf ellipticals hosting strong radio AGNs. C1 [Miller, Neal A.; Hornschemeier, Ann E.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Hornschemeier, Ann E.] NASA, Goddard Space Flight Ctr, Lab Xray Astrophys, Greenbelt, MD 20771 USA. [Mobasher, Bahram] Univ Calif Riverside, Dept Phys & Astron, Riverside, CA 92521 USA. [Bridges, Terry J.] Anglo Australian Observ, Epping, NSW 1710, Australia. [Bridges, Terry J.] Queens Univ, Dept Phys, Kingston, ON K7L 3N6, Canada. [Hudson, Michael J.] Univ Waterloo, Dept Phys & Astron, Waterloo, ON N2L 3G1, Canada. [Marzke, Ronald O.] San Francisco State Univ, Dept Phys & Astron, San Francisco, CA 94132 USA. [Smith, Russell J.] Univ Durham, Dept Phys, Durham DH1 3LE, England. RP Miller, NA (reprint author), Johns Hopkins Univ, Dept Phys & Astron, 3400 N Charles St, Baltimore, MD 21218 USA. EM nmiller@pha.jhu.edu RI Hudson, Michael/H-3238-2012 OI Hudson, Michael/0000-0002-1437-3786 NR 77 TC 13 Z9 13 U1 0 U2 2 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 MAY PY 2009 VL 137 IS 5 BP 4450 EP 4467 DI 10.1088/0004-6256/137/5/4450 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 430WB UT WOS:000265019900026 ER PT J AU Perrin, MD Vacca, WD Graham, JR AF Perrin, Marshall D. Vacca, William D. Graham, James R. TI EVIDENCE FOR AN EDGE-ON DISK AROUND THE YOUNG STAR MWC 778 FROM INFRARED IMAGING AND POLARIMETRY SO ASTRONOMICAL JOURNAL LA English DT Article DE circumstellar matter; planetary systems: protoplanetary disks; stars: individual (MWC 778); stars: pre-main sequence ID HERBIG-AE/BE STARS; T-TAURI STARS; H-II REGIONS; ADAPTIVE OPTICS; CIRCUMSTELLAR DISK; IRAS SOURCES; PLANETARY-NEBULAE; SOLAR CIRCLE; CALIBRATION; EVOLUTION AB MWC 778 is an unusual and little-studied young stellar object located in the IC 2144 nebula. Recent spectroscopy by Herbig & Vacca suggested the presence of an edge-on circumstellar disk around it. We present near-infrared adaptive optics imaging polarimetry and mid-infrared imaging which directly confirm the suspected nearly edge-on disk around MWC 778 (i similar to 70 degrees-80 degrees) plus reveal a more extensive envelope pierced by bipolar outflow cavities. In addition, our mid-infrared images and near-infrared polarization maps detect a spiral-shaped structure surrounding MWC 778, with arms that extend beyond 6 '' on either side of the star. Although MWC 778 has previously been classified as a Herbig Ae/Be star, the properties of its central source (including its spectral type) remain fairly uncertain. Herbig & Vacca suggested an F or G spectral type based on the presence of metallic absorption lines in the optical spectrum, which implies that MWC 778 may belong to the fairly rare class of intermediate-mass T Tauri Stars (IMTTSs) which are the evolutionary precursors to Herbig Ae/Be objects. Yet its integrated bolometric luminosity, greater than or similar to 750 L(circle dot) (for an assumed distance of 1 kpc) is surprisingly high for an F or G spectral type, even for an IMTTS. We speculate on several possible explanations for this discrepancy, including its true distance being much closer than 1 kpc, the presence of a binary companion, and/or a nonstellar origin for the observed absorption lines. C1 [Perrin, Marshall D.] Univ Calif Los Angeles, Div Astron, Los Angeles, CA 90095 USA. [Vacca, William D.] NASA, Ames Res Ctr, SOFIA USRA, Moffett Field, CA 94035 USA. [Graham, James R.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Perrin, Marshall D.; Graham, James R.] Univ Calif Santa Cruz, Ctr Adapt Opt, Santa Cruz, CA 95064 USA. RP Perrin, MD (reprint author), Univ Calif Los Angeles, Div Astron, Los Angeles, CA 90095 USA. EM mperrin@ucla.edu; wvacca@sofia.usra.edu; jrg@berkeley.edu FU NASA; NSF FX W. D. V. thanks George Herbig for calling his attention to this source and for numerous discussions regarding its nature, and also thanks Goeran Sandell for his insight regarding Herbig Ae/ Be stars. M. D. P. thanks John Monnier for useful discussions. These observations were made possible by the dedicated and hard working staffs of the Lick and Gemini Observatories, and in particular M. D. P. is most grateful for expert assistance from Elinor Gates, R. Scott Fisher, and Kevin Volk. The data presented here were obtained as part of a thesis project by M. D. P., who was supported at that time by a NASA Michelson Graduate Fellowship administered by JPL, and is now supported by a NSF Astronomy & Astrophysics Postdoctoral Fellowship. J. R. G. and M. D. P. were supported in part by the National Science Foundation Science and Technology Center for AdaptiveOptics, managed by theUniversity of California at Santa Cruz under cooperative agreement AST-9876783. NR 41 TC 5 Z9 5 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 MAY PY 2009 VL 137 IS 5 BP 4468 EP 4477 DI 10.1088/0004-6256/137/5/4468 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 430WB UT WOS:000265019900027 ER PT J AU Brown, PJ Holland, ST Immler, S Milne, P Roming, PWA Gehrels, N Nousek, J Panagia, N Still, M Berk, DV AF Brown, Peter J. Holland, Stephen T. Immler, Stefan Milne, Peter Roming, Peter W. A. Gehrels, Neil Nousek, John Panagia, Nino Still, Martin Berk, Daniel Vanden TI ULTRAVIOLET LIGHT CURVES OF SUPERNOVAE WITH THE SWIFT ULTRAVIOLET/OPTICAL TELESCOPE SO ASTRONOMICAL JOURNAL LA English DT Article DE distance scale; dust, extinction; galaxies: distances and redshifts; supernovae: general; ultraviolet: general ID X-RAY OBSERVATIONS; HUBBLE-SPACE-TELESCOPE; IA SUPERNOVAE; PHOTOMETRIC IDENTIFICATION; OPTICAL OBSERVATIONS; SYNTHETIC SPECTRA; UVOT OBSERVATIONS; SHOCK BREAKOUT; SN 1993J; GRB-060218 AB We present ultraviolet (UV) observations of supernovae (SNe) obtained with the UltraViolet/Optical Telescope (UVOT) on board the Swift spacecraft. This is the largest sample of UV light curves from any single instrument and covers all major SN types and most subtypes. The UV light curves of SNe Ia are fairly homogenous, while SNe Ib/c and IIP show more variety in their light-curve shapes. The UV-optical colors clearly differentiate SNe Ia and IIP, particularly at early times. The color evolution of SNe IIP, however, makes their colors similar to SNe Ia at about 20 days after explosion. SNe Ib/c are shown to have varied UV-optical colors. The use of UV colors to help type SNe will be important for high-redshift SNe discovered in optical observations. These data can be added to ground-based optical and near infrared data to create bolometric light curves of individual objects and as checks on generic bolometric corrections used in the absence of UV data. This sample can also be compared with rest-frame UV observations of high-redshift SNe observed at optical wavelengths. C1 [Brown, Peter J.; Roming, Peter W. A.; Nousek, John; Berk, Daniel Vanden] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Holland, Stephen T.; Immler, Stefan; Gehrels, Neil] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20770 USA. [Holland, Stephen T.] Univ Space Res Assoc, Columbia, MD 21044 USA. [Holland, Stephen T.; Immler, Stefan] NASA, Goddard Space Flight Ctr, Ctr Res & Explorat Space Sci & Technol, Greenbelt, MD 20770 USA. [Milne, Peter] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Panagia, Nino] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Panagia, Nino] Osserv Astrofis Catania, INAF, I-95128 Catania, Italy. [Panagia, Nino] Supernova Ltd, Virgin Gorda, British Virgin, England. [Still, Martin] Univ Coll London, Mullard Space Sci Lab, Dept Space & Climate Phys, Dorking RH5 6NT, Surrey, England. RP Brown, PJ (reprint author), Penn State Univ, Dept Astron & Astrophys, 525 Davey Lab, University Pk, PA 16802 USA. RI Gehrels, Neil/D-2971-2012 FU NASA [NAS5-00136]; Swift Guest Investigator grant [NNH06ZDA001N] FX This work made use of public data from the Swift data archive. This work is supported at Penn State by NASA Contract NAS5-00136 and Swift Guest Investigator grant NNH06ZDA001N. NR 72 TC 85 Z9 85 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 J9 ASTRON J JI Astron. J. PD MAY PY 2009 VL 137 IS 5 BP 4517 EP 4525 DI 10.1088/0004-6256/137/5/4517 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 430WB UT WOS:000265019900030 ER PT J AU Pottasch, SR Bernard-Salas, J Roellig, TL AF Pottasch, S. R. Bernard-Salas, J. Roellig, T. L. TI Abundances in the planetary nebula NGC 6210 SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE ISM: abundances; planetary nebulae: individual: NGC6210; infrared: ISM; stars: evolution ID SPITZER-SPACE-TELESCOPE; OPTICAL RECOMBINATION LINES; GIANT BRANCH STARS; INFRARED SPECTROGRAPH; CHEMICAL ABUNDANCES; STELLAR EVOLUTION; MASS-LOSS; 4.85 GHZ; TEMPERATURE; CATALOG AB The spectra of the planetary nebula NGC6210 is reanalysed using spectral measurements made in the mid-infrared with the Spitzer Space Telescope and the Infrared Space Observatory. The aim is to determine the chemical composition of this object. We also make use of IUE and ground based spectra. Abundances determined from the mid-infrared lines, which are insensitive to electron temperature, are used as the basis for the determination of the composition, which is found to differ somewhat from earlier results. The abundances found, especially the low value of helium and oxygen, indicate that the central star was originally of rather low mass, probably <= 1 M(circle dot). Abundances of phosphorus, iron, silicon, sodium, potassium and chlorine have been determined, some for the first time in this nebula. The electron temperature in this nebula is constant. The temperature, radius and luminosity of the central star is also discussed. It is shown that the luminosity is consistent with that predicted for a star of 0.9 M(circle dot). But the predicted nebular age is inconsistent with the observed kinetic age. C1 [Pottasch, S. R.] Univ Groningen, Kapteyn Astron Inst, NL-9700 AV Groningen, Netherlands. [Bernard-Salas, J.] Cornell Univ, Ctr Radiophys & Space Res, Ithaca, NY 14853 USA. [Roellig, T. L.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Pottasch, SR (reprint author), Univ Groningen, Kapteyn Astron Inst, POB 800, NL-9700 AV Groningen, Netherlands. EM pottasch@astro.rug.nl FU Jet Propulsion Laboratory, California Institute of Technology under NASA [1407]; NASA [1257184] FX This work is based on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology under NASA contract 1407. Support for this work was provided by NASA through Contract Number 1257184 issued by JPL/Caltech. NR 33 TC 10 Z9 10 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 MAY PY 2009 VL 499 IS 1 BP 249 EP 256 DI 10.1051/0004-6361/200911654 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 448UD UT WOS:000266286600022 ER PT J AU Guidorzi, C Clemens, C Kobayashi, S Granot, J Melandri, A D'Avanzo, P Kuin, NPM Klotz, A Fynbo, JPU Covino, S Greiner, J Malesani, D Mao, J Mundell, CG Steele, IA Jakobsson, P Margutti, R Bersier, D Campana, S Chincarini, G D'Elia, V Fugazza, D Genet, F Gomboc, A Kruhler, T Yoldas, AK Moretti, A Mottram, CJ O'Brien, PT Smith, RJ Szokoly, G Tagliaferri, G Tanvir, NR Gehrels, N AF Guidorzi, C. Clemens, C. Kobayashi, S. Granot, J. Melandri, A. D'Avanzo, P. Kuin, N. P. M. Klotz, A. Fynbo, J. P. U. Covino, S. Greiner, J. Malesani, D. Mao, J. Mundell, C. G. Steele, I. A. Jakobsson, P. Margutti, R. Bersier, D. Campana, S. Chincarini, G. D'Elia, V. Fugazza, D. Genet, F. Gomboc, A. Kruehler, T. Yoldas, A. Kuepcue Moretti, A. Mottram, C. J. O'Brien, P. T. Smith, R. J. Szokoly, G. Tagliaferri, G. Tanvir, N. R. Gehrels, N. TI Rise and fall of the X-ray flash 080330: an off-axis jet? SO ASTRONOMY & ASTROPHYSICS LA English DT Review DE gamma rays: bursts; X-rays: individual: XRF 080330 ID AFTERGLOW LIGHT CURVES; BURST ALERT TELESCOPE; LORENTZ FACTOR; E-P,E-I-E-ISO CORRELATION; SWIFT OBSERVATIONS; SPECTRAL CATALOG; 2-COMPONENT JET; CENTRAL ENGINE; EMISSION; MODELS AB Context. X-ray flashes (XRFs) are a class of gamma-ray bursts (GRBs) with a peak energy of the time-integrated. F. spectrum, E-p, typically below 30 keV, whereas classical GRBs have Ep of a few hundreds of keV. Apart from Ep and the systematically lower luminosity, the properties of XRFs, such as their duration or spectral indices, are typical of the classical GRBs. Yet, the nature of XRFs and their differences from GRBs are not understood. In addition, there is no consensus on the interpretation of the shallow decay phase observed in most X-ray afterglows of both XRFs and GRBs. Aims. We examine in detail the case of XRF 080330 discovered by Swift at redshift 1.51. This burst is representative of the XRF class and exhibits an X-ray shallow decay. The rich broadband (from NIR to UV) photometric data set we collected during this phase makes it an ideal candidate for testing the off-axis jet interpretation proposed to explain both the softness of XRFs and the shallow decay phase. Methods. We present prompt gamma-ray, early and late NIR/visible/UV and X-ray observations of the XRF 080330. We derive a spectral energy distribution from NIR to X-ray bands across the shallow/plateau phase and describe the temporal evolution of the multiwavelength afterglow within the context of the standard afterglow model. Results. The multiwavelength evolution of the afterglow is achromatic from similar to 10(2) s to similar to 8 x 10(4) s. The energy spectrum from NIR to X-ray is reproduced well by a simple power-law, F-v proportional to v(-beta ox), with beta(ox) = 0.79 +/- 0.01 and negligible rest-frame dust extinction. The light curve can be modelled by either a piecewise power-law or the combination of a smoothly broken power law with an initial rise up to similar to 600 s, a plateau lasting up to similar to 2 ks, followed by a gradual steepening to a power-law decay index of similar to 2 until 82 ks. At this point, a bump appears to be modelled well with a second component, while the corresponding optical energy spectrum, F-v proportional to v(-beta o), reddens Delta beta(o) = 0.26 +/- 0.06. Conclusions. A single-component jet viewed off-axis can explain the light curve of XRF 080330, the late-time reddening being due to the reverse shock of an energy injection episode and its being an XRF. Other possibilities, such as the optical rise marking the pre-deceleration of the fireball within a wind environment, cannot be excluded definitely, but appear to be contrived. We exclude the possibility of a dust decreasing column density being swept up by the fireball as explaining the rise of the afterglow. C1 [Guidorzi, C.; D'Avanzo, P.; Covino, S.; Mao, J.; Margutti, R.; Campana, S.; Chincarini, G.; Fugazza, D.; Moretti, A.; Tagliaferri, G.] INAF Osservatorio Astron Brera, I-23807 Merate, LC, Italy. [Guidorzi, C.; Kobayashi, S.; Melandri, A.; Mundell, C. G.; Steele, I. A.; Bersier, D.; Mottram, C. J.; Smith, R. J.] Liverpool John Moores Univ, Astrophys Res Inst, Birkenhead CH41 1LD, Merseyside, England. [Guidorzi, C.] Univ Ferrara, Dipartimento Fis, I-44100 Ferrara, Italy. [Clemens, C.; Greiner, J.; Kruehler, T.; Yoldas, A. Kuepcue; Szokoly, G.] Max Planck Inst Extraterr Phys, D-85740 Garching, Germany. [Granot, J.; Genet, F.] Univ Hertfordshire, Ctr Astrophys Res, Hatfield AL10 9AB, Herts, England. [Kuin, N. P. M.] Univ Coll London, Mullard Space Sci Lab, Dorking RH5 6NT, Surrey, England. [Klotz, A.] Observ Haute Provence, F-04870 St Michel lObservatoire, France. [Klotz, A.] Univ Toulouse, CNRS, CESR, Observ Midi Pyrenees, F-31028 Toulouse 04, France. [Fynbo, J. P. U.; Malesani, D.] Univ Copenhagen, Niels Bohr Inst, Dark Cosmol Ctr, DK-2100 Copenhagen O, Denmark. [Mao, J.] Chinese Acad Sci, Natl Astron Observ, Yunnan Observ, Kunming 650011, Yunnan Province, Peoples R China. [Jakobsson, P.] Univ Iceland, Inst Sci, Ctr Astrophys & Cosmol, IS-107 Reykjavik, Iceland. [Margutti, R.; Chincarini, G.] Univ Milano Bicocca, Dipartimento Fis, I-20126 Milan, Italy. [D'Elia, V.] INAF Osservatorio Astron Roma, I-00040 Monte Porzio Catone, RM, Italy. [Gomboc, A.] Univ Ljubljana, Fac Math & Phys, Ljubljana 1000, Slovenia. [O'Brien, P. T.; Tanvir, N. R.] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England. [Gehrels, N.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Guidorzi, C (reprint author), INAF Osservatorio Astron Brera, Via E Bianchi 46, I-23807 Merate, LC, Italy. EM guidorzi@fe.infn.it RI Gehrels, Neil/D-2971-2012; Fynbo, Johan/L-8496-2014; Jakobsson, Pall/L-9950-2015; OI Fynbo, Johan/0000-0002-8149-8298; Jakobsson, Pall/0000-0002-9404-5650; Campana, Sergio/0000-0001-6278-1576; D'Elia, Valerio/0000-0002-7320-5862; moretti, alberto/0000-0002-9770-0315; Covino, Stefano/0000-0001-9078-5507; Kruehler, Thomas/0000-0002-8682-2384; Tagliaferri, Gianpiero/0000-0003-0121-0723 FU ASI [I/R/039/04]; Ministry of University and Research of Italy [PRIN 2005025417]; Royal Society Wolfson Research Merit Award; DNRF; Marie Curie European Re-integration [PERG03-GA-2008-226653]; Icelandic Research Fund FX This work is supported by ASI grant I/R/039/04 and by the Ministry of University and Research of Italy (PRIN 2005025417). J. G. gratefully acknowledges a Royal Society Wolfson Research Merit Award. DARK is funded by the DNRF. P. J. acknowledges support by a Marie Curie European Re-integration Grant within the 7th European Community Framework Program under contract number PERG03-GA-2008-226653, and a Grant of Excellence from the Icelandic Research Fund. We gratefully acknowledge the contribution of the Swift team members at OAB, PSU, UL, GSFC, ASDC, MSSL and our sub-contractors, who helped make this mission possible. We acknowledge Sami-Matias Niemi for executing the NOT observations. CG is grateful to A. Kann for his reading and comments. NR 128 TC 35 Z9 35 U1 1 U2 9 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 MAY PY 2009 VL 499 IS 2 BP 439 EP U108 DI 10.1051/0004-6361/200911719 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 455BJ UT WOS:000266730500010 ER PT J AU Spezzi, L Pagano, I Marino, G Leto, G Young, E Siegler, N Balog, Z Messina, S Distefano, E Merin, B Navascues, DBY AF Spezzi, L. Pagano, I. Marino, G. Leto, G. Young, E. Siegler, N. Balog, Z. Messina, S. Distefano, E. Merin, B. Barrado y Navascues, D. TI A deep multi-band investigation of IC 2391 SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE stars: formation; stars: low-mass, brown dwarfs; stars: pre-main sequence; stars: circumstellar matter; ISM: individual objects: IC 2391 ID LOW-MASS STARS; SPITZER-SPACE-TELESCOPE; BROWN DWARF CANDIDATES; OPEN CLUSTER IC-2391; MAIN-SEQUENCE STARS; INFRARED ARRAY CAMERA; YOUNG OPEN CLUSTERS; LITHIUM-DEPLETION; ABSOLUTE CALIBRATION; INTERSTELLAR CLOUDS AB Aims. We report the outcome of a deep multiwavelength study of the IC 2391 young open cluster. We attempt to uncover new low-mass and sub-stellar members of the cluster and identify new debris disk objects. Methods. We observed a 30 x 30 square arcmin area in IC 2391 using the wide-field imager at the ESO 2.2m telescope. The completeness limits of the photometry at the 3 sigma level are V = 24.7, R(C) = 23.7, and I(C) = 23.0, faint enough to reveal sub-stellar members down to similar to 0.03 M(circle dot). Our membership criteria are based on use of our optical data in combination with JHK(S) magnitudes from the 2MASS catalog. We also estimate the physical parameters of the selected candidates. Debris disk candidates are identified on the basis of their infrared excess emission using near- and mid-infrared photometry from the Spitzer Space Telescope. Results. Our optical survey, which has a limiting magnitude at the 3 sigma level 1-2 mag fainter than previous optical surveys conducted in IC 2391, revealed 29 new low-mass member candidates of the cluster. We estimate the contamination to be at least similar to 50%. We constrain the fraction of sub-stellar objects in the range 8-15% and discuss possible explanations of the deficit of brown dwarfs in this cluster. We also identify 10 candidates in the cluster showing IR excess emission consistent with the presence of debris disks. C1 [Spezzi, L.; Pagano, I.; Marino, G.; Leto, G.; Messina, S.; Distefano, E.] INAF Osservatorio Astrofis Catania, I-95123 Catania, Italy. [Spezzi, L.] European Space Agcy ESTEC, NL-2200 AG Noordwijk, Netherlands. [Young, E.; Balog, Z.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Siegler, N.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Barrado y Navascues, D.] European Space Agcy ESAC, Ctr Astrobiol, LAEFF, CAB,INTA,CSIC,Lab Astrofis Espacial & Exoplanetas, Madrid 28691, Spain. RP Spezzi, L (reprint author), INAF Osservatorio Astrofis Catania, Via S Sofia 78, I-95123 Catania, Italy. EM lspezzi@rssd.esa.int RI Leto, Giuseppe/N-3355-2015; Pagano, Isabella/I-6934-2015; Barrado Navascues, David/C-1439-2017; OI Leto, Giuseppe/0000-0002-0040-5011; Pagano, Isabella/0000-0001-9573-4928; Merin, Bruno/0000-0002-8555-3012; Barrado Navascues, David/0000-0002-5971-9242; Distefano, Elisa/0000-0002-2448-2513; Messina, Sergio/0000-0002-2851-2468 FU European Southern Observatory, La Silla (Chile) [68.D-0541(A)] FX This paper is based on observations carried out at the European Southern Observatory, La Silla (Chile), under observing program number 68.D-0541(A). This publication makes use of data products from the Two Micron All Sky Survey, which is a joint project of the University of Massachusetts and the Infrared Processing and Analysis Center/California Institute of Technology, funded by NASA and the National Science Foundation. We also acknowledge extensive use of the SIMBAD database, operated at CDS Strasbourg, the WEBDA database, operated at the Institute for Astronomy of the University of Vienna, and the NOMAD catalog, released by the U. S. Naval Observatory. L. Spezzi acknowledges financial support from INAF-Catania. We thank J.M.Alcala, A. Frasca, D. Gandolfi and F. Comeron for many discussions and suggestions. We are also grateful to many others, in particular to Salvatore Spezzi. NR 95 TC 5 Z9 5 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 MAY PY 2009 VL 499 IS 2 BP 541 EP 555 DI 10.1051/0004-6361/200810609 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 455BJ UT WOS:000266730500019 ER PT J AU Farinelli, R Paizis, A Landi, R Titarchuk, L AF Farinelli, R. Paizis, A. Landi, R. Titarchuk, L. TI The X-ray spectral evolution of Cygnus X-2 in the framework of bulk Comptonization SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE stars: individual: Cygnus X-2; stars: neutron; X-rays: binaries; accretion, accretion disks ID MONTE-CARLO SIMULATIONS; ACCRETING NEUTRON-STARS; IRON-K LINE; BLACK-HOLE; GX 17+2; OBSERVATIONAL EVIDENCE; FREQUENCY CORRELATION; ASTRONOMY SATELLITE; ENERGY-SPECTRA; SCORPIUS X-1 AB Context. Strong theoretical and observational support exists that the spectral evolution of neutron-star LMXBs, including transient hard X-ray tails, can be explained by the interplay between thermal and bulk motion Comptonization. The introduction of a new XSPEC Comptonization model, COMPTB, including thermal and bulk Comptonization, has provided additional support to this interpretation. Aims. We used COMPTB to investigate the spectral evolution of the neutron-star LMXB Cyg X-2 along its Z track. We selected a single source to trace in a quantitative way the evolution of the physical parameters of the model. Methods. We analyzed archival broad-band BeppoSAX spectra of Cyg X-2. Five broad-band spectra were newly extracted by using information about the source position in the Z track described in the colour-colour and colour-intensity diagrams. Results. We fitted the spectra of the source with two COMPTB components. The first one, with a bulk parameter delta = 0, represents the dominant component of the overall source broad-band spectrum and its origin is related to thermal upscattering (Comptonization) of cold seed photons by warm electrons in a high opacity enviroment. We attribute the origin of these seed photons to the section of the disk that illuminates the outer coronal region (transition layer) located between the accretion disk itself and the neutron-star surface. The physical properties of this thermal component are roughly constant with both time and inferred mass accretion rate. The second COMPTB model describes the overall Comptonization (thermal plus bulk, delta > 0) of hotter seed photons that originate in both the inner transition layer and at the neutron-star surface. This component is more significant in the horizontal branch of the colour-colour or hardness-intensity diagram and progressively disappears towards the normal branch, where a pure blackbody spectrum is observed. Conclusions. The spectral evolution of Cyg X-2 is studied and interpreted in terms of changes in the innermost environmental conditions of the system, leading to a variable thermal-bulk Comptonization efficiency. C1 [Farinelli, R.; Titarchuk, L.] Univ Ferrara, Dipartmento Fis, I-44100 Ferrara, Italy. [Paizis, A.] INAF IASF, Sez Milano, I-20133 Milan, Italy. [Landi, R.] INAF IASF, Sez Bologna, I-40100 Bologna, Italy. [Titarchuk, L.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Farinelli, R (reprint author), Univ Ferrara, Dipartmento Fis, Via Saragat 1, I-44100 Ferrara, Italy. EM farinelli@fe.infn.it OI Paizis, Adamantia/0000-0001-5067-0377 FU Italian Space Agency [I/008/07/0]; Italian PRIN-INAF FX The authors are very grateful to the anonymous referee, whose suggestions strongly improved the quality of the paper with respect to the formerly submitted version. A. P. acknowledges the Italian Space Agency financial and programmatic support via contract I/008/07/0. This work has been partially supported by the grant from Italian PRIN-INAF 2007, "Bulk motion Comptonization models in X-ray Binaries: from phenomenology to physics", PI M. Cocchi. NR 56 TC 10 Z9 10 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 MAY PY 2009 VL 498 IS 2 BP 509 EP 516 DI 10.1051/0004-6361/200810422 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 442VL UT WOS:000265868600026 ER PT J AU Butters, OW Norton, AJ Mukai, K Barlow, EJ AF Butters, O. W. Norton, A. J. Mukai, K. Barlow, E. J. TI RXTE confirmation of the intermediate polar status of IGR J15094-6649 SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE stars: binaries: general; stars: novae, cataclysmic variables; stars: individual: IGR J15094-6649; X-rays: binaries AB Aims. We aim to establish the X-ray properties of the intermediate polar candidate IGR J15094-6649 and therefore confirm its inclusion into the class. Methods. 42 856 s of X-ray data from RXTE was analysed. Frequency analysis was used to constrain temporal variations and spectral analysis used to characterise the emission and absorption properties. Results. A spin period of 809.7 +/- 0.6 s is present, revealed as a complex pulse profile whose modulation depth decreases with increasing X-ray energy. The spectrum is well fitted by either a 17 +/- 4 keV Bremsstrahlung or Gamma = 1.8 +/- 0.1 power law, with an iron emission line feature and significant absorption in each case. Conclusions. IGR J15094-6649 is confirmed to be an intermediate polar. C1 [Butters, O. W.] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England. [Butters, O. W.; Norton, A. J.; Barlow, E. J.] Open Univ, Dept Phys & Astron, Milton Keynes MK7 6AA, Bucks, England. [Mukai, K.] NASA GSFC, CRESST & Xray Astrophys Lab, Greenbelt, MD 20771 USA. [Mukai, K.] Univ Maryland, Dept Phys, Baltimore, MD 21250 USA. RP Butters, OW (reprint author), Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England. EM oliver.butters@star.le.ac.uk OI Norton, Andrew/0000-0001-7619-8269; Butters, Olly/0000-0003-0354-8461 NR 12 TC 5 Z9 5 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 MAY PY 2009 VL 498 IS 2 BP L17 EP L19 DI 10.1051/0004-6361/200911725 PG 3 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 442VL UT WOS:000265868600003 ER PT J AU Zatsepin, VI Panov, AD Sokolskaya, NV Adams, JH Ahn, HS Bashindzhagyan, GL Chang, J Christl, M Fazely, AR Guzik, TG Isbert, JB Kim, KC Kouznetsov, EN Panasyuk, M Seo, ES Watts, J Wefel, JP Wu, J AF Zatsepin, V. I. Panov, A. D. Sokolskaya, N. V. Adams, J. H., Jr. Ahn, H. S. Bashindzhagyan, G. L. Chang, J. Christl, M. Fazely, A. R. Guzik, T. G. Isbert, J. B. Kim, K. C. Kouznetsov, E. N. Panasyuk, M. Seo, E. S. Watts, J. Wefel, J. P. Wu, J. TI Energy dependence of Ti/Fe ratio in the Galactic cosmic rays measured by the ATIC-2 experiment SO ASTRONOMY LETTERS-A JOURNAL OF ASTRONOMY AND SPACE ASTROPHYSICS LA English DT Article DE cosmic rays; cosmic ray propagation ID REACCELERATION AB Titanium is a rare, secondary nucleus among Galactic cosmic rays. Using the Silicon matrix in the ATIC experiment, Titanium has been separated. The energy dependence of the Ti to Fe flux ratio in the energy region from 5 GeV per nucleon to about 500 GeV per nucleon is presented. C1 [Zatsepin, V. I.; Panov, A. D.; Sokolskaya, N. V.; Bashindzhagyan, G. L.; Panasyuk, M.] Moscow MV Lomonosov State Univ, Skobeltsyn Inst Nucl Phys, Moscow, Russia. [Adams, J. H., Jr.; Christl, M.; Kouznetsov, E. N.; Watts, J.] NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA. [Ahn, H. S.; Kim, K. C.; Seo, E. S.; Wu, J.] Univ Maryland, College Pk, MD 20742 USA. [Chang, J.] Acad Sinica, Purple Mt Observ, Nanjing 210008, Peoples R China. [Fazely, A. R.] Southern Univ, Baton Rouge, LA USA. [Guzik, T. G.; Isbert, J. B.; Wefel, J. P.] Louisiana State Univ, Baton Rouge, LA 70803 USA. RP Zatsepin, VI (reprint author), Moscow MV Lomonosov State Univ, Skobeltsyn Inst Nucl Phys, Moscow, Russia. EM viza@dec1.sinp.ms RI Panasyuk, Mikhail/E-2005-2012; Zatsepin, Victor/J-2287-2012; Sokolskaya, Natalia/J-4609-2012; Panov, Alexander/K-3952-2012; OI Panov, Alexander/0000-0003-2290-6498; Seo, Eun-Suk/0000-0001-8682-805X FU Russian Foundation for Basic Reseach [05-02-16222]; National Aeronautics and Space Administration of the United States [NNG04WC12G, NNG04WC10G, NNG04WC06G] FX This work was supported by the Russian Foundation for Basic Reseach (grant no. 05-02-16222) and the National Aeronautics and Space Administration of the United States (grants nos. NNG04WC12G, NNG04WC10G, and NNG04WC06G). NR 12 TC 8 Z9 8 U1 0 U2 3 PU MAIK NAUKA/INTERPERIODICA/SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013-1578 USA SN 1063-7737 J9 ASTRON LETT+ JI Astron. Lett.-J. Astron. Space Astrophys. PD MAY PY 2009 VL 35 IS 5 BP 338 EP 342 DI 10.1134/S1063773709050089 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 444EA UT WOS:000265962100008 ER PT J AU Serabyn, E Mawet, D Bloemhof, E Haguenauer, P Mennesson, B Wallace, K Hickey, J AF Serabyn, E. Mawet, D. Bloemhof, E. Haguenauer, P. Mennesson, B. Wallace, K. Hickey, J. TI IMAGING FAINT BROWN DWARF COMPANIONS CLOSE TO BRIGHT STARS WITH A SMALL, WELL-CORRECTED TELESCOPE APERTURE SO ASTROPHYSICAL JOURNAL LA English DT Article DE instrumentation: adaptive optics; stars: low-mass, brown dwarfs ID PHASE-MASK CORONAGRAPH; ADAPTIVE OPTICS SURVEY; DESERT; LIMITS AB We have used our 1.6 m diameter off-axis well-corrected subaperture (WCS) on the Palomar Hale telescope in concert with a small inner-working-angle phase-mask coronagraph to image the immediate environs of a small number of nearby stars. Test cases included three stars (HD 130948, HD 49197, and HR7672) with known brown dwarf companions at small separations, all of which were detected. We also present the initial detection of a new object close to the nearby young G0V star HD171488. Follow-up observations are needed to determine if this object is a bona fide companion, but its flux is consistent with the flux of a young brown dwarf or low-mass M star at the same distance as the primary. Interestingly, at small angles our WCS coronagraph demonstrates a limiting detectable contrast comparable to that of extant Lyot coronagraphs on much larger telescopes corrected with current-generation adaptive optics (AO) systems. This suggests that small apertures corrected to extreme AO (ExAO) levels can be used to carry out initial surveys for close brown dwarf and stellar companions, leaving follow-up observations for larger telescopes. C1 [Serabyn, E.; Mawet, D.; Bloemhof, E.; Haguenauer, P.; Mennesson, B.; Wallace, K.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Hickey, J.] CALTECH, Palomar Observ, Palomar Mt, CA 92060 USA. RP Serabyn, E (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. FU National Aeronautics and Space Administration FX This work was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration, and is based in part on observations obtained at the Hale Telescope, Palomar Observatory, as part of a continuing collaboration between the California Institute of Technology, NASA/JPL, and Cornell University. We thank M. Troy and the JPL AO team, and the staff of the Palomar Observatory for their able and ready assistance. NR 32 TC 14 Z9 14 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAY 1 PY 2009 VL 696 IS 1 BP 40 EP 46 DI 10.1088/0004-637X/696/1/40 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 435NH UT WOS:000265350100004 ER PT J AU Sokolov, IV Roussev, II Skender, M Gombosi, TI Usmanov, AV AF Sokolov, Igor V. Roussev, Ilia I. Skender, Marina Gombosi, Tamas I. Usmanov, Arcadi V. TI TRANSPORT EQUATION FOR MHD TURBULENCE: APPLICATION TO PARTICLE ACCELERATION AT INTERPLANETARY SHOCKS SO ASTROPHYSICAL JOURNAL LA English DT Article DE acceleration of particles; MHD; shock waves; Sun: coronal mass ejections (CMEs); turbulence; waves ID NONMONOCHROMATIC ALFVEN-WAVE; SOLAR-WIND; MAGNETOHYDRODYNAMIC TURBULENCE; PARAMETRIC-INSTABILITY; COSMIC-RAYS; ATMOSPHERE; EVOLUTION; DRIVEN; FRONTS; MODEL AB The aim of the present paper is to unify the various transport equations for turbulent waves that are used in different areas of space physics. Here, we mostly focus on the magnetohydrodynamic turbulence, in particular the Alfvenic turbulence. The applied methods, however, are general and can be extended to other forms of turbulence, for example the acoustic turbulence, or Langmuir plasma waves. With minor modifications, the derivations followed here can be extended for relativistic motions, thus making it possible to apply them to the wave transport in astrophysical objects with high plasma speeds (radiojets), or strong gravity (black hole surroundings). C1 [Sokolov, Igor V.; Gombosi, Tamas I.] Univ Michigan, Dept AOSS, Ann Arbor, MI 48109 USA. [Roussev, Ilia I.; Skender, Marina] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. [Usmanov, Arcadi V.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Sokolov, IV (reprint author), Univ Michigan, Dept AOSS, 2455 Hayward St, Ann Arbor, MI 48109 USA. EM igorsok@umich.edu; iroussev@ifa.hawaii.edu; tamas@umich.edu; Arcadi.Usmanov.1@gsfc.nasa.gov RI Roussev, Ilia/E-9141-2011; Gombosi, Tamas/G-4238-2011; Usmanov, Arcadi/A-9860-2013; Sokolov, Igor/H-9860-2013 OI Gombosi, Tamas/0000-0001-9360-4951; Sokolov, Igor/0000-0002-6118-0469 FU NSF [ATM-0454469, ATM-0631790, ATM-0639335]; NASA-LWS [NNG05GM70G, NNX07AC13G]; Bulgarian NSF [VU-NZ-01/06] FX The authors thank an unknown referee for the useful comments made on the manuscript. We are also grateful to G. Li, C. Smith, J. Le Roux, and G. Zank for the productive discussions on the subject matter. This research work was supported by NSF grants ATM-0454469 (FDSS), ATM-0631790 (SHINE), and ATM-0639335 (CAREER), as well as NASA-LWS grants NNG05GM70G and NNX07AC13G. I. R. would like to acknowledge the limited support received from grant VU-NZ-01/06 with the Bulgarian NSF. NR 24 TC 16 Z9 16 U1 0 U2 8 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAY 1 PY 2009 VL 696 IS 1 BP 261 EP 267 DI 10.1088/0004-637X/696/1/261 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 435NH UT WOS:000265350100024 ER PT J AU Soria, R Ghosh, KK AF Soria, Roberto Ghosh, Kajal K. TI DIFFERENT TYPES OF ULTRALUMINOUS X-RAY SOURCES IN NGC 4631 SO ASTROPHYSICAL JOURNAL LA English DT Article DE black hole physics; X-rays: binaries; X-rays: individual (NGC 4631) ID XMM-NEWTON OBSERVATIONS; MASS BLACK-HOLES; MULTIPHASE GASEOUS HALOS; NEARBY SPIRAL GALAXIES; ACCRETION DISKS; SPECTRAL PROPERTIES; EXTERNAL GALAXIES; STAR-FORMATION; H-ALPHA; HOT GAS AB We have re-examined the most luminous X-ray sources in the starburst galaxy NGC 4631, using XMM-Newton, Chandra, and ROSAT data. The most interesting source is a highly variable supersoft ultraluminous X-ray source (ULX). We suggest that its bolometric luminosity similar to a few 10(39) erg s(-1) in the high/supersoft state: this is an order of magnitude lower than estimated in previous studies, thus reducing the need for extreme or exotic scenarios. Moreover, we find that this source was in a noncanonical low/soft (kT similar to 0.1-0.3 keV) state during the Chandra observation. By comparing the high and low state, we argue that the spectral properties may not be consistent with the expected behavior of an accreting intermediate-mass black hole. We suggest that recurrent super-Eddington outbursts with photospheric expansion from a massive white dwarf (M(wd) greater than or similar to 1.3 M(circle dot)), powered by nonsteady nuclear burning, may be a viable possibility, in alternative to the previously proposed scenario of a super-Eddington outflow from an accreting stellar-mass black hole. The long-term average accretion rate required for nuclear burning to power such white-dwarf outbursts in this source and perhaps in other supersoft ULXs is approximate to (5-10) x 10(-6) M(circle dot) yr(-1): this is comparable to the thermal-timescale mass transfer rate invoked to explain the most luminous hard-spectrum ULXs ( powered by black hole accretion). The other four most luminous X-ray sources in NGC 4631 ( three of which can be classified as ULXs) appear to be typical accreting black holes, in four different spectral states: high/soft, convex-spectrum, power-law with soft excess, and simple power-law. None of them require masses greater than or similar to 50 M(circle dot). C1 [Soria, Roberto] Univ Coll London, Mullard Space Sci Lab, Dorking RH5 6NT, Surrey, England. [Ghosh, Kajal K.] NASA, George C Marshall Space Flight Ctr, Univ Space Res Assoc, Huntsville, AL 35805 USA. RP Soria, R (reprint author), Univ Coll London, Mullard Space Sci Lab, Holmbury St Mary, Dorking RH5 6NT, Surrey, England. EM roberto.soria@mssl.ucl.ac.uk FU NASA [NNG04GC86G]; Space Telescope Science Institute [HST/AR-10954]; Leverhulme Fellowship; UK-China Fellowship; Tsinghua University FX We thank the referee for a thoughtful review and interesting suggestions which have considerably improved the paper. This research has made use of the NASA/IPAC Extragalactic Database (NED) which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with NASA; and from the Chandra Data Archive, part of the Chandra X-Ray Observatory Science Center (CXC) which is operated for NASA by SAO. Support for this research was provided in part by NASA under Grant NNG04GC86G issued through the Office of Space Science and from the Space Telescope Science Institute under the grant HST/AR-10954. R. S. acknowledges support from a Leverhulme Fellowship, a UK-China Fellowship for excellence, and from Tsinghua University (Beijing). We thank Kinwah Wu, Shaung-Nan Zhang, and Xin-Lin Zhou for their comments and discussions. NR 58 TC 13 Z9 13 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAY 1 PY 2009 VL 696 IS 1 BP 287 EP 297 DI 10.1088/0004-637X/696/1/287 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 435NH UT WOS:000265350100028 ER EF