FN Thomson Reuters Web of Science™ VR 1.0 PT J AU Hathaway, DH Wilson, RM AF Hathaway, David H. Wilson, Robert M. TI Geomagnetic activity indicates large amplitude for sunspot cycle 24 SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID SOLAR-CYCLE; DYNAMO AB The level of geomagnetic activity near the time of solar activity minimum has been shown to be a reliable indicator for the amplitude of the following solar activity maximum. The geomagnetic activity index aa can be split into two components: one associated with solar flares, prominence eruptions, and coronal mass ejections which follows the solar activity cycle and a second component associated with recurrent high speed solar wind streams which is out of phase with the solar activity cycle. This second component often peaks before solar activity minimum and has been one of the most reliable indicators for the amplitude of the following maximum. The size of the recent maximum in this second component indicates that solar activity cycle 24 will be much higher than average - similar in size to cycles 21 and 22 with a peak smoothed sunspot number of 160 +/- 25. C1 NASA, Natl Space Sci & Technol Ctr, Huntsville, AL 35812 USA. RP Hathaway, DH (reprint author), NASA, Natl Space Sci & Technol Ctr, MC VP62, Huntsville, AL 35812 USA. EM david.hathaway@nasa.gov NR 13 TC 77 Z9 78 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 SEP 16 PY 2006 VL 33 IS 18 AR L18101 DI 10.1029/2006GL027053 PG 3 WC Geosciences, Multidisciplinary SC Geology GA 085ZO UT WOS:000240643100003 ER PT J AU Sonnabend, G Sornig, M Krotz, PJ Schieder, RT Fast, KE AF Sonnabend, G. Sornig, M. Kroetz, P. J. Schieder, R. T. Fast, K. E. TI High spatial resolution mapping of Mars mesospheric zonal winds by infrared heterodyne spectroscopy of CO2 SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID MARTIAN ATMOSPHERE; NATURAL LASER; EMISSION; VENUS; SPECTROMETER; BANDS; MODEL AB We present Mars zonal wind measurements by means of infrared heterodyne spectroscopy of CO2 features at 959.3917 cm(-1) (10.423 mu m). Observations were carried out using the Cologne Tuneable Heterodyne Infrared Spectrometer (THIS) from 5 - 8 December 2005 shortly after Mars opposition at the McMath-Pierce Solar Telescope of the National Solar Observatory on Kitt Peak in Arizona with an unprecedented spatial resolution of similar to 1.7 arcsec on a similar to 16 arcsec Martian disk. Mars was observed at six different latitudes close to the west ( evening) limb and zonal winds were retrieved from Doppler shifts between CO2 non-thermal emission from the mesosphere and absorption features from low atmospheric regions. The season on Mars was late northern winter (L-S approximate to 337 degrees). We retrieved retrograde winds at latitude 45 degrees N ( - 27 +/- 17 m/s) that were particularly strong at the equator ( up to - 80 +/- 13 m/s) and prograde winds at high southern latitudes ( 75 degrees S) up to 51 +/- 29 m/s. C1 Univ Cologne, Inst Phys 1, D-50937 Cologne, Germany. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Sonnabend, G (reprint author), Univ Cologne, Inst Phys 1, D-50937 Cologne, Germany. EM samstag@ph1.uni-koeln.de NR 23 TC 18 Z9 18 U1 0 U2 3 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD SEP 16 PY 2006 VL 33 IS 18 AR L18201 DI 10.1029/2006GL026900 PG 5 WC Geosciences, Multidisciplinary SC Geology GA 085ZO UT WOS:000240643100001 ER PT J AU Forbes, JM Russell, J Miyahara, S Zhang, X Palo, S Mlynczak, M Mertens, CJ Hagan, ME AF Forbes, J. M. Russell, J. Miyahara, S. Zhang, X. Palo, S. Mlynczak, M. Mertens, C. J. Hagan, M. E. TI Troposphere-thermosphere tidal coupling as measured by the SABER instrument on TIMED during July-September 2002 SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article ID NONMIGRATING DIURNAL TIDES; GENERAL-CIRCULATION MODEL; LATENT-HEAT RELEASE; MIDDLE ATMOSPHERE; SEMIDIURNAL TIDES; PLANETARY-WAVES; MLT REGION; GLOBAL DISTRIBUTIONS; HOUGH COMPONENTS; SOLAR TIDES AB [ 1] Coupling between the troposphere and lower thermosphere due to upward propagating tides is investigated using temperatures measured from the SABER instrument on the TIMED satellite. The data analyzed here are confined to 20 - 120 km altitude and +/- 40 degrees latitude during 20 July to 20 September 2002. Apart from the migrating (Sun-synchronous) tidal components, the predominant feature seen ( from the satellite frame) during this period is a wave-4 structure in longitude with extrema of up to +/- 40 - 50 K at 110 km. Amplitudes and longitudes of maxima of this structure evolve as the satellite precesses in local time and as the wave(s) responsible for this structure vary with time. The primary wave responsible for the wave-4 pattern is the eastward propagating diurnal tide with zonal wave number s = 3 (DE3). Its average amplitude distribution over the interval is quasi-symmetric about the equator, similar to that of a Kelvin wave, with maximum of about 20 K at 5 degrees S and 110 km. DE3 is primarily excited by latent heating due to deep tropical convection in the troposphere. It is demonstrated that existence of DE3 is intimately connected with the predominant wave-4 longitude distribution of topography and land-sea difference at low latitudes, and an analogy is drawn with the strong presence of DE1 in Mars atmosphere, the predominant wave-2 topography on Mars, and the wave-2 patterns that dominate density measurements from the Mars Global Surveyor (MGS) spacecraft near 130 km. Additional diurnal, semidiurnal, and terdiurnal nonmigrating tides are also revealed in the present study. These tidal components are most likely excited by nonlinear interactions between their migrating counterparts and the stationary planetary wave with s = 1 known to exist in the Southern Hemisphere during this period just prior to the austral midwinter stratospheric warming of 2002. C1 Univ Colorado, Dept Aerosp Engn Sci, Boulder, CO 80309 USA. Hampton Univ, Ctr Atmospher Sci, Hampton, VA 23668 USA. Kyushu Univ, Dept Earth & Planetary Sci, Fukuoka 8128581, Japan. NASA, Langley Res Ctr, Hampton, VA 23681 USA. Natl Ctr Atmospher Res, High Altitude Observ, Boulder, CO 80307 USA. RP Forbes, JM (reprint author), Univ Colorado, Dept Aerosp Engn Sci, UCB 429, Boulder, CO 80309 USA. EM forbes@colorado.edu RI Hagan, Maura/C-7200-2008; Mlynczak, Martin/K-3396-2012; U-ID, Kyushu/C-5291-2016; OI Hagan, Maura/0000-0002-8866-7429; FORBES, JEFFREY/0000-0001-6937-0796; PALO, SCOTT/0000-0002-4729-4929 NR 62 TC 102 Z9 103 U1 0 U2 6 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9380 EI 2169-9402 J9 J GEOPHYS RES-SPACE JI J. Geophys. Res-Space Phys. PD SEP 16 PY 2006 VL 111 IS A10 AR A10S06 DI 10.1029/2005JA011492 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 086BR UT WOS:000240648600001 ER PT J AU Green, JL Boardsen, S Garcia, L Fung, SF Reinisch, BW AF Green, James L. Boardsen, Scott Garcia, Leonard Fung, Shing F. Reinisch, B. W. TI Reply to "Comment on "On the origin of whistler mode radiation in the plasmasphere'' by Green et al.'' SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Editorial Material ID HISS C1 NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. NASA, Goddard Space Flight Ctr, Commun Analyt Div L3, Greenbelt, MD 20771 USA. NASA, Goddard Space Flight Ctr, QSS Grp Inc, Greenbelt, MD 20771 USA. Univ Massachusetts, Ctr Atmospher Res, Lowell, MA 01854 USA. RP Green, JL (reprint author), NASA, Goddard Space Flight Ctr, Code 603, Greenbelt, MD 20771 USA. EM james.green@nasa.gov RI Fung, Shing/F-5647-2012 NR 11 TC 14 Z9 14 U1 0 U2 0 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 SEP 16 PY 2006 VL 111 IS A9 AR A09211 DI 10.1029/2006JA011622 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 086BK UT WOS:000240647900006 ER PT J AU Podesta, JJ Roberts, DA Goldstein, ML AF Podesta, J. J. Roberts, D. A. Goldstein, M. L. TI Self-similar scaling of magnetic energy in the inertial range of solar wind turbulence SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article ID FLOWS AB Turbulent magnetic field fluctuations in the solar wind undergo an energy cascade in the inertial range with a characteristic Kolmogorov frequency spectrum f(-5/3). Using magnetic field measurements from the Wind and ACE spacecraft at 1 AU in the ecliptic plane, probability distributions (PDFs) of time-delayed differences of magnetic energy density B-2(t) are shown to exhibit an approximate self-similar scaling for time lags tau in the inertial range of the turbulence, that is, from approximately 10 to 1000 s. The scaling is characterized by a single scaling exponent gamma, the Hurst exponent, and a universal PDF that is independent of scale for timescales in the inertial range. It is shown that the scaling exponent and the form of the universal PDF change with the 11-year solar cycle due to the changing nature of the turbulence. The timescale for these changes is roughly estimated to be on the order of 1 or 2 years. Studies of low-order structure functions are performed in an attempt to corroborate the self-similar scaling of the PDFs. It is found that the structure functions do not scale in a self-similar manner indicating that the PDFs are not truly self-similar. Therefore the claimed self-similar scaling of the PDFs is only a rough approximation. C1 NASA, Goddard Space Flight Ctr, Lab Solar & Space Phys, Greenbelt, MD 20771 USA. RP Podesta, JJ (reprint author), NASA, Goddard Space Flight Ctr, Lab Solar & Space Phys, Code 612-2, Greenbelt, MD 20771 USA. EM jpodesta@solar.stanford.edu RI Roberts, Dana/D-4625-2012; Goldstein, Melvyn/B-1724-2008 NR 13 TC 9 Z9 9 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 SEP 16 PY 2006 VL 111 IS A9 AR A09105 DI 10.1029/2006JA011766 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 086BK UT WOS:000240647900010 ER PT J AU Cantrell, JH AF Cantrell, John H. TI Dependence of microelastic-plastic nonlinearity of martensitic stainless steel on fatigue damage accumulation SO JOURNAL OF APPLIED PHYSICS LA English DT Article ID ACOUSTIC HARMONIC-GENERATION; PERSISTENT SLIP BANDS; DISLOCATION-STRUCTURES; ELASTIC-CONSTANTS; COPPER; BEHAVIOR; MICROSTRUCTURES; ORGANIZATION; DIPOLES; METALS AB Self-organized substructural arrangements of dislocations formed during cyclic stress-induced fatigue of metals produce substantial changes in the material microelastic-plastic nonlinearity, a quantitative measure of which is the nonlinearity parameter beta extracted from acoustic harmonic generation measurements. The contributions to beta from the substructural evolution of dislocations and crack growth for fatigued martensitic 410Cb stainless steel are calculated from the Cantrell model [Proc. R. Soc. London, Ser. A 460, 757 (2004)] as a function of percent full fatigue life to fracture. A wave interaction factor f(WI) is introduced into the model to account experimentally for the relative volume of fatigue damage included in the total volume of material swept out by an interrogating acoustic wave. For cyclic stress-controlled loading at 551 MPa and f(WI)=0.013 the model predicts a monotonic increase in beta from dislocation substructures of almost 100% from the virgin state to roughly 95% full life. Negligible contributions from cracks are predicted in this range of fatigue life. However, during the last 5% of fatigue life the model predicts a rapid monotonic increase of beta by several thousand percent that is dominated by crack growth. The theoretical predictions are in good agreement with experimental measurements of 410Cb stainless steel samples fatigued in uniaxial, stress-controlled cyclic loading at 551 MPa from zero to full tensile load with a measured f(WI) of 0.013. (c) 2006 American Institute of Physics. C1 NASA, Langley Res Ctr, Hampton, VA 23681 USA. RP Cantrell, JH (reprint author), NASA, Langley Res Ctr, Mail Stop 231, Hampton, VA 23681 USA. EM john.h.cantrell@nasa.gov NR 30 TC 27 Z9 28 U1 1 U2 10 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 SEP 15 PY 2006 VL 100 IS 6 AR 063508 DI 10.1063/1.2345614 PG 7 WC Physics, Applied SC Physics GA 089JL UT WOS:000240876600027 ER PT J AU Troupaki, E Vasilyev, AA Kashem, NB Allan, GR Stephen, MA AF Troupaki, Elisavet Vasilyev, Aleksey A. Kashem, Nasir B. Allan, Graham R. Stephen, Mark A. TI Space qualification and environmental testing of quasicontinuous wave laser diode arrays SO JOURNAL OF APPLIED PHYSICS LA English DT Article AB NASA's mission requirements for spaceborne laser diode arrays lead to a set of tests peculiar to space flight. The goal of these tests is to determine if vibration, radiation, or vacuum will impair the operation or lifetime of nominally 100 W quasicontinuous wave 808 nm laser diode arrays. To simulate the stresses expected during a mission, terrestrial tests involve mechanical vibration, simulating the acceleration of launch, exposure to the equivalent doses of ionizing radiation, and operation in a vacuum. Three sets of devices were tested: one set with random vibration up to 20 g root-mean-square (grms) applied along three axes, a second set of devices was irradiated with gamma radiation (1.17 and 1.33 MeV) at 744 rad(Si)/min up to 200 krad(Si), and the third set was exposed to a flux of 5x10(11) or 10(12) p/cm(2) of 200 MeV protons up to 60 krad total dose. Only the proton irradiated devices showed any effect attributable to the test: a slight rise in lasing threshold, which recovered over time with self-annealing. A selection of the devices were then operated in vacuum for a further 1400 h accumulating 500x10(6) pulses without any signs of degradation. Similar results were obtained in a parallel test, conducted in air, accumulating over 10(9) pulses on a selection of the remaining devices. (c) 2006 American Institute of Physics. C1 Sci Syst & Applicat Inc, Lanham, MD 20706 USA. NASA, Goddard Space Flight Ctr, Laser & Electro Opt Branch, Greenbelt, MD 20771 USA. Sigma Space Corp, Lanham, MD 20706 USA. RP Troupaki, E (reprint author), Sci Syst & Applicat Inc, Lanham, MD 20706 USA. EM elisavet_troupaki@ssaihq.com RI Allan, Graham/D-3905-2013 NR 13 TC 10 Z9 10 U1 0 U2 3 PU AMER INST PHYSICS PI MELVILLE PA CIRCULATION & FULFILLMENT DIV, 2 HUNTINGTON QUADRANGLE, STE 1 N O 1, MELVILLE, NY 11747-4501 USA SN 0021-8979 J9 J APPL PHYS JI J. Appl. Phys. PD SEP 15 PY 2006 VL 100 IS 6 AR 063109 DI 10.1063/1.2353795 PG 5 WC Physics, Applied SC Physics GA 089JL UT WOS:000240876600009 ER PT J AU Seevaratnam, GK Walker, LM Rame, E Garoff, S AF Seevaratnam, G. K. Walker, L. M. Rame, E. Garoff, S. TI Wetting by simple room-temperature polymer melts: Deviations from Newtonian behavior (vol 284, pg 265, 2005) SO JOURNAL OF COLLOID AND INTERFACE SCIENCE LA English DT Correction C1 Carnegie Mellon Univ, Ctr Complex Fluids Engn, Pittsburgh, PA 15213 USA. Carnegie Mellon Univ, Dept Chem Engn, Pittsburgh, PA 15213 USA. Carnegie Mellon Univ, Dept Phys, Pittsburgh, PA 15213 USA. NASA, Glenn Res Ctr, Natl Ctr Micrograv Res, Cleveland, OH 44135 USA. RP Garoff, S (reprint author), Carnegie Mellon Univ, Ctr Complex Fluids Engn, Pittsburgh, PA 15213 USA. EM sg2e@andrew.cmu.edu RI Garoff, Stephen/P-7629-2014; Walker, Lynn/I-2562-2016 OI Garoff, Stephen/0000-0001-8148-8535; Walker, Lynn/0000-0002-7478-9759 NR 1 TC 0 Z9 0 U1 2 U2 3 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0021-9797 J9 J COLLOID INTERF SCI JI J. Colloid Interface Sci. PD SEP 15 PY 2006 VL 301 IS 2 BP 706 EP 706 DI 10.1016/j.jcis.2006.06.032 PG 1 WC Chemistry, Physical SC Chemistry GA 076DR UT WOS:000239937700050 ER PT J AU Churilov, A Ostrogorsky, AG Volz, MP AF Churilov, A. Ostrogorsky, A. G. Volz, M. P. TI Solidification using a baffle in sealed ampoules: Ground-based experiments SO JOURNAL OF CRYSTAL GROWTH LA English DT Article DE characterization; directional solidification; segregation; microgravity conditions; semiconducting III v materials ID SUBMERGED HEATER METHOD; DIRECTIONAL SOLIDIFICATION; VERTICAL BRIDGMAN; CRYSTAL-GROWTH; SEGREGATION; CONVECTION; INSB; MICROGRAVITY; GRAVITY; GA AB Six InSb crystals doped with Te or Zn were grown to provide the reference data for the analysis of the space experiments conducted at the International Space Station within the solidification using a baffle in sealed ampoules (SUBSA) investigation. The dopant concentration was measured using the Hall Effect, 4-point probe and Atomic Absorption methods. The dopant segregation profiles in all crystals grown on Earth demonstrate the presence of strong convective mixing in the melt. (c) 2006 Elsevier B.V. All rights reserved. C1 Rensselaer Polytech Inst, Mech Aeronaut & Nucl Engn Dept, Troy, NY 12180 USA. NASA, Marshall Space Flight Ctr, Huntsville, AL 35812 USA. RP Ostrogorsky, AG (reprint author), Rensselaer Polytech Inst, Mech Aeronaut & Nucl Engn Dept, 110 8th St,2026 JEC Bldg, Troy, NY 12180 USA. EM ostroa@rpi.edu NR 26 TC 2 Z9 2 U1 1 U2 2 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 SEP 15 PY 2006 VL 295 IS 1 BP 20 EP 30 DI 10.1016/j.jcrysgro.2006.07.024 PG 11 WC Crystallography; Materials Science, Multidisciplinary; Physics, Applied SC Crystallography; Materials Science; Physics GA 093OR UT WOS:000241178100005 ER PT J AU Weitz, CM Anderson, RC Bell, JF Farrand, WH Herkenhoff, KE Johnson, JR Jolliff, BL Morris, RV Squyres, SW Sullivan, RJ AF Weitz, C. M. Anderson, R. C. Bell, J. F., III Farrand, W. H. Herkenhoff, K. E. Johnson, J. R. Jolliff, B. L. Morris, R. V. Squyres, S. W. Sullivan, R. J. TI Soil grain analyses at Meridiani Planum, Mars SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Article ID ROVER LANDING SITE; OPPORTUNITY ROVER; MICROSCOPIC IMAGER; BURNS FORMATION; GUSEV CRATER; SPECTROMETER; MINERALOGY; CHEMISTRY; EVOLUTION; HEMATITE AB [ 1] Grain-size analyses of the soils at Meridiani Planum have been used to identify rock sources for the grains and provide information about depositional processes under past and current conditions. Basaltic sand, dust, millimeter-size hematite-rich spherules interpreted as concretions, spherule fragments, coated partially buried spherules, basalt fragments, sedimentary outcrop fragments, and centimeter-size cobbles are concentrated on the upper surfaces of the soils as a lag deposit, while finer basaltic sands and dust dominate the underlying soils. There is a bimodal distribution of soil grain sizes with one population representing grains < 125 mu m and the other falling between 1 - 4.5 mm. Soils within craters like Eagle and Endurance show a much greater diversity of grain morphologies compared to the plains. The spherules found in the plains soils are approximately 1 - 2 mm smaller in size than those seen embedded in the outcrop rocks of Eagle and Endurance craters. The average major axis for all unfractured spherules measured in the soils and outcrop rocks is 2.87 +/- 1.18 mm, with a trend toward decreasing spherule sizes in both the soils and outcrop rocks as the rover drove southward. Wind ripples seen across the plains of Meridiani are dominated by similar size (1.3 - 1.7 mm) hematite-rich grains, and they match in size the larger grains on plains ripples at Gusev Crater. Larger clasts and centimeter-size cobbles that are scattered on the soils have several spectral and compositional types, reflecting multiple origins. The cobbles tend to concentrate within ripple troughs along the plains and in association with outcrop exposures. C1 Planetary Sci Inst, Tucson, AZ 85719 USA. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. Cornell Univ, Dept Astron, Ithaca, NY 14853 USA. Space Sci Inst, Boulder, CO 80301 USA. US Geol Survey, Flagstaff, AZ 86001 USA. Washington Univ, Dept Earth & Planetary Sci, St Louis, MO 63130 USA. NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. RP Weitz, CM (reprint author), Planetary Sci Inst, 1700 E Ft Lowell,Suite 106, Tucson, AZ 85719 USA. EM weitz@psi.edu RI Johnson, Jeffrey/F-3972-2015 NR 32 TC 42 Z9 42 U1 1 U2 5 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9097 EI 2169-9100 J9 J GEOPHYS RES-PLANET JI J. Geophys. Res.-Planets PD SEP 15 PY 2006 VL 111 IS E12 AR E12S04 DI 10.1029/2005JE002541 PG 26 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 086AU UT WOS:000240646300001 ER PT J AU Huang, FT Mayr, HG Reber, CA Killeen, T Russell, J Mlynczak, M Skinner, W Mengel, J AF Huang, Frank T. Mayr, Hans G. Reber, Carl A. Killeen, Timothy Russell, James Mlynczak, Marty Skinner, Wilbert Mengel, John TI Diurnal variations of temperature and winds inferred from TIMED and UARS measurements SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article ID DOPPLER-SPREAD PARAMETERIZATION; ATMOSPHERE RESEARCH SATELLITE; GENERAL-CIRCULATION MODEL; WAVE MOMENTUM DEPOSITION; LONG-TERM VARIABILITY; LARGE-SCALE DYNAMICS; MIDDLE ATMOSPHERE; GRAVITY-WAVE; LOWER THERMOSPHERE; PLANETARY-WAVES AB Owing to their sampling properties in local solar time, both the TIMED and UARS spacecrafts provide the opportunity to quantitatively study the mesospheric thermal tides. The information though is limited because it takes the TIMED instruments 2 months to cover the full range of 24 hours, almost twice as long as UARS. We present here the results of an analysis, in which the seasonal and global-scale variations of amplitude and phase for the migrating diurnal tide are retrieved from atmospheric temperature and wind measurements on the TIMED (SABER, TIDI) and UARS (MLS, HRDI) satellites. Comparisons are made with results from the Numerical Spectral Model (NSM), which is characterized in part by the parameterization of small-scale gravity waves. At 60 km and above, the amplitude and phase variations of the diurnal tide from the NSM agree generally well with those derived from the SABER temperatures. In the SABER temperature amplitudes at around 60 km there are evident asymmetries in latitude with respect to the equator, which are not apparent in the MLS data near 55 km or in the NSM. (The asymmetry in the SABER temperatures disappears above 60 km.) For the meridional winds of the migrating diurnal tide derived from TIDI, the phase and relative amplitude variation with latitude and season are in qualitative agreement with the HRDI measurements and the NSM. The amplitudes from TIDI winds are systematically smaller, but this may in part be due to interannual variations. However, the results for the zonal winds from TIDI more often do not agree well with those from HRDI or the NSM. C1 Creat Comp Solut Inc, Rockville, MD 20850 USA. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Natl Ctr Atmospher Res, High Altitude Observ, Boulder, CO 80307 USA. NASA, Langley Res Ctr, Hampton, VA 23681 USA. Hampton Univ, Ctr Atmospher Sci, Hampton, VA 23668 USA. Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA. Sci Syst & Applicat, Lanham, MD 20706 USA. RP Huang, FT (reprint author), Creat Comp Solut Inc, Rockville, MD 20850 USA. EM fthuang@comcast.net RI Mlynczak, Martin/K-3396-2012 NR 49 TC 22 Z9 22 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 SEP 15 PY 2006 VL 111 IS A10 AR A10S04 DI 10.1029/2005JA011426 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 086BP UT WOS:000240648400001 ER PT J AU Ray, CS Reis, ST Pontuschka, WM Yang, JB Sene, FF Giehl, JM Kim, CW Sen, S AF Ray, C. S. Reis, S. T. Pontuschka, W. M. Yang, J. B. Sene, F. F. Giehl, J. M. Kim, C. W. Sen, S. TI Mossbauer and EPR spectra for glasses and glass-ceramics prepared from simulated compositions of Lunar and Martian soils SO JOURNAL OF NON-CRYSTALLINE SOLIDS LA English DT Article; Proceedings Paper CT 7th Brazilian Symposium on Glasses and Related Materials/3rd International Symposium on Non-Crystalline Solids in Brazil CY NOV 13-16, 2005 CL Maringa, BRAZIL SP Natl Council Sci & Technol Dev, CNPq, Brazilian Innvovat Agcy, FINEP, CAPES Fdn, Parana Fdn, Fund Araucar DE composition; crystallization; glass ceramics; glass melting; glass formation; glass transition; magnetic properties; Mossbauer effect and spectroscopy; X-rays; X-ray diffraction ID ELECTRON-PARAMAGNETIC-RESONANCE; IRON PHOSPHATE-GLASSES; IONS AB In situ resource processing and utilization on planetary bodies is an important and integral part of NASA's space exploration program. Within this scope and context, our general effort is primarily aimed at developing glass and glass-ceramic type materials using Lunar and Martian soils, and exploring various application potentials of these materials for planetary surface operations. This paper reports the successful preparation of glasses from the melts of simulated composition of Lunar and Martian soils, and thermal and structural characterization using differential thermal analysis (DTA), Mossbauer and electron paramagnetic resonance (EPR) spectroscopy. Glass-ceramic materials were developed from these glasses using selective heat treatment, and were also analyzed by Mossbauer and EPR spectroscopy. The crystalline phases formed at different stages of heat treatment were analyzed and identified by X-ray diffraction (XRD). Potential applications envisaged up to this time of these glasses/glass-ceramics on the surface of Moon or Mars are discussed. (c) 2006 Elsevier B.V. All rights reserved. C1 NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA. Univ Missouri, Mat Res Ctr, Rolla, MO 65409 USA. Univ Sao Paulo, Inst Phys, BR-05315970 Sao Paulo, Brazil. Inst Nucl Energy Res, BR-05422970 Sao Paulo, Brazil. NASA, George C Marshall Space Flight Ctr, BAE Syst, Huntsville, AL 35812 USA. RP Ray, CS (reprint author), NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA. EM Chandra.S.Ray@nasa.gov; reis@umr.edu RI Pontuschka, Walter/I-4934-2012 NR 19 TC 5 Z9 5 U1 0 U2 4 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0022-3093 J9 J NON-CRYST SOLIDS JI J. Non-Cryst. Solids PD SEP 15 PY 2006 VL 352 IS 32-35 BP 3677 EP 3684 DI 10.1016/j.jnoncrysol.2006.02.117 PG 8 WC Materials Science, Ceramics; Materials Science, Multidisciplinary SC Materials Science GA 086XI UT WOS:000240706000054 ER PT J AU Sztul, HI Kartazayev, V Alfano, RR AF Sztul, H. I. Kartazayev, V. Alfano, R. R. TI Laguerre-Gaussian supercontinuum SO OPTICS LETTERS LA English DT Article ID ORBITAL ANGULAR-MOMENTUM; OPTICAL VORTICES; LIGHT; BEAMS AB We show what is believed to be the first coherent white-light optical vortices generated from supercontinuum that have the azimuthally varying phase structure consistent with a monochromatic Laguerre-Gaussian beam. Two methods of Laguerre-Gaussian supercontinuum. generation are discussed and contrasted. We use a computer-generated hologram to convert a Gaussian white-light supercontinuum source into Laguerre-Gaussian supercontinuum. (c) 2006 Optical Society of America. C1 CUNY, Inst Ultrfast Spect & Lasers,NASA, Ctr Opt Sensing & Imaging,Dept Phys, New York, NY 10031 USA. CUNY, Grad Sch, City Coll, New York, NY 10031 USA. RP Sztul, HI (reprint author), CUNY, Inst Ultrfast Spect & Lasers,NASA, Ctr Opt Sensing & Imaging,Dept Phys, 160 Convent Ave, New York, NY 10031 USA. EM hsztul@gc.cuny.edu NR 14 TC 17 Z9 17 U1 1 U2 5 PU OPTICAL SOC AMER PI WASHINGTON PA 2010 MASSACHUSETTS AVE NW, WASHINGTON, DC 20036 USA SN 0146-9592 J9 OPT LETT JI Opt. Lett. PD SEP 15 PY 2006 VL 31 IS 18 BP 2725 EP 2727 DI 10.1364/OL.31.002725 PG 3 WC Optics SC Optics GA 083GN UT WOS:000240444500020 PM 16936871 ER PT J AU Brock, JC Wright, CW Kuffner, IB Hernandez, R Thompson, P AF Brock, John C. Wright, C. Wayne Kuffner, Ilsa B. Hernandez, Raquel Thompson, Philip TI Airborne lidar sensing of massive stony coral colonies on patch reefs in the northern Florida reef tract SO REMOTE SENSING OF ENVIRONMENT LA English DT Article DE coral reefs; remote sensing; lidar; videography AB In this study we examined the ability of the NASA Experimental Advanced Airborne Research Lidar (EAARL) to discriminate cluster zones of massive stony coral colonies on northern Florida reef tract (NFRT) patch reefs based on their topographic complexity (rugosity). Spatially dense EAARL laser submarine topographic soundings acquired in August 2002 were used to create a 1-m resolution digital rugosity map for adjacent NFRT study areas characterized by patch reefs (Region A) and diverse substratums (Region B). In both regions, sites with lidar-sensed rugosities above 1.2 were imaged by an along-track underwater videography system that incorporated the acquisition of instantaneous GPS positions. Subsequent manual interpretation of videotape segments was performed to identify substratum types that caused elevated lidar-sensed rugosity. Our study determined that massive coral colony formation, modified by subsequent physical and biological processes that breakdown patch reef framework, was the primary source of topographic complexity sensed by the EAARL in the NFRT. Sites recognized by lidar scanning to be topographically complex preferentially occurred around the margins of patch reefs, constituted a minor fraction of the reef system, and usually reflected the presence of massive coral colonies in cluster zones, or their derivatives created by mortality, bioerosion, and physical breakdown. (c) 2006 Elsevier Inc. All rights reserved. C1 US Geol Survey, St Petersburg, FL 33701 USA. NASA, Goddard Space Flight Ctr, Wallops Isl Flight Facil, Wallops Isl, VA 23337 USA. Nova SE Univ, Natl Coral Reef Inst, Dania, FL 33004 USA. RP Brock, JC (reprint author), US Geol Survey, 600 4th St S, St Petersburg, FL 33701 USA. EM jbrock@usgs.gov RI Kuffner, Ilsa/A-6416-2008; OI Kuffner, Ilsa/0000-0001-8804-7847 NR 29 TC 42 Z9 44 U1 0 U2 12 PU ELSEVIER SCIENCE INC PI NEW YORK PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA SN 0034-4257 J9 REMOTE SENS ENVIRON JI Remote Sens. Environ. PD SEP 15 PY 2006 VL 104 IS 1 BP 31 EP 42 DI 10.1016/j.rse.2006.04.017 PG 12 WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic Technology SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science & Photographic Technology GA 081ZZ UT WOS:000240357400003 ER PT J AU White, MA Nemani, RR AF White, Michael A. Nemani, Ramakrishna R. TI Real-time monitoring and short-term forecasting of land surface phenology SO REMOTE SENSING OF ENVIRONMENT LA English DT Article DE growing season; budburst; bud break; senescence; spring; fall ID LEAF-AREA INDEX; SATELLITE DATA; REGIONS; AVHRR; MODEL; MODIS; NDVI; USA AB Land surface phenology is an important process for real-time monitoring and short-term forecasting in diverse land management, health, and hydrologic modeling applications. Yet current efforts to characterize phenological processes are limited by remote sensing challenges and lack of uncertainty estimates. Here, for a global distribution of phenologically and climatically similar phenoregions, we used the Advanced Very High Resolution Radiometer to develop a conceptually and computationally simple technique for real-time and forecast applications. Our overall approach was to analyze the phenological behavior of groups of pixels without recourse to smoothing or fitting. We used a 3-step initial process: (1) define a phenoregion specific normalized difference vegetation index threshold; (2) for all days from 19822003, calculate the percent of pixels above the threshold (PAT); (3) calculate daily 1982-2003 empirical distributions of PAT. For real-time monitoring, the current PAT may then be compared to the historical range of variability and visualized in relation to user-defined levels. Using similar concepts, we projected daily PAT up to one month in the future and compared predicted and actual dates at which a hypothetical PAT was reached. We found that the maximum lead-time of phenological forecasts could be analytically defined for user-specified uncertainty levels. The approach is adaptable to different remote sensing technologies and provides a foundation for ascribing a sequence of ground conditions (e.g. snowmelt, vegetative growth, pollen production, insect phenology) to remotely sensed land surface phenology observations. (c) 2006 Elsevier Inc. All rights reserved. C1 Utah State Univ, Dept Aquat Watershed & Earth Resources, Logan, UT 84322 USA. NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP White, MA (reprint author), Utah State Univ, Dept Aquat Watershed & Earth Resources, Logan, UT 84322 USA. OI White, Michael/0000-0002-0238-8913 NR 27 TC 88 Z9 96 U1 4 U2 35 PU ELSEVIER SCIENCE INC PI NEW YORK PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA SN 0034-4257 EI 1879-0704 J9 REMOTE SENS ENVIRON JI Remote Sens. Environ. PD SEP 15 PY 2006 VL 104 IS 1 BP 43 EP 49 DI 10.1016/j.rse.2006.04.014 PG 7 WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic Technology SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science & Photographic Technology GA 081ZZ UT WOS:000240357400004 ER PT J AU Min, QL Lin, B AF Min, Qilong Lin, Bing TI Determination of spring onset and growing season leaf development using satellite measurements SO REMOTE SENSING OF ENVIRONMENT LA English DT Article DE spring onset detection; growing season duration; microwave remote sensing; emissivity difference vegetation index (EDVI); leaf development ID MICROWAVE EMISSION; VEGETATION INDEXES; DECIDUOUS FOREST; SOIL-MOISTURE; UNITED-STATES; AREA INDEX; REFLECTANCE; TEMPERATURE; RADIOMETER; RADIATION AB SAn integrated approach to retrieve microwave emissivity difference vegetation index (EDVI) over land regions has been developed from combined multi-platform/multi-sensor satellite measurements, including SSM/I measurements. A possible relationship of the remotely sensed EDVI and the leaf physiology of canopy is explored at the Harvard Forest site for two growing seasons. This study finds that the EDVI is sensitive to leaf development through vegetation water content of the crown layer of the forest canopy, and has demonstrated that the spring onset and growing season duration can be determined accurately from the time series of satellite estimated EDVI within uncertainties of approximately 3 and 7 days for spring onset and growing season duration, respectively, compared to in situ observations. The leaf growing stage can also be monitored by a normalized EDVI. EDVI retrievals from satellite generally are possible during both daytime and nighttime when it is not raining. The EDVI technique studied here may provide higher temporal resolution observations for monitoring the onset of spring, the duration of growing season, and leaf development stage compared to current operational satellite methods. (c) 2006 Elsevier Inc. All rights reserved. C1 SUNY Albany, Atmospher Sci Res Ctr, Albany, NY 12222 USA. NASA, Langley Res Ctr, Sci Directorate, Hampton, VA 23665 USA. RP Min, QL (reprint author), SUNY Albany, Atmospher Sci Res Ctr, Albany, NY 12222 USA. EM min@asrc.cestm.albany.edu NR 29 TC 14 Z9 15 U1 0 U2 5 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 SEP 15 PY 2006 VL 104 IS 1 BP 96 EP 102 DI 10.1016/j.rse.2006.05.006 PG 7 WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic Technology SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science & Photographic Technology GA 081ZZ UT WOS:000240357400009 ER PT J AU Flasar, FM AF Flasar, F. M. TI Titan's polar weather SO SCIENCE LA English DT Editorial Material ID CLOUDS; VORTEX; STRATOSPHERE; TEMPERATURE; ATMOSPHERE; DYNAMICS C1 NASA, Goddard Space Flight Ctr, Planetary Syst Lab, Greenbelt, MD 20771 USA. RP Flasar, FM (reprint author), NASA, Goddard Space Flight Ctr, Planetary Syst Lab, Greenbelt, MD 20771 USA. EM f.m.flasar@nasa.gov RI Flasar, F Michael/C-8509-2012 NR 15 TC 5 Z9 6 U1 0 U2 1 PU AMER ASSOC ADVANCEMENT SCIENCE PI WASHINGTON PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 USA SN 0036-8075 J9 SCIENCE JI Science PD SEP 15 PY 2006 VL 313 IS 5793 BP 1582 EP 1583 DI 10.1126/science.1130698 PG 2 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 083YS UT WOS:000240498900028 PM 16973865 ER PT J AU Griffith, CA Penteado, P Rannou, P Brown, R Boudon, V Baines, KH Clark, R Drossart, P Buratti, B Nicholson, P McKay, CP Coustenis, A Negrao, A Jaumann, R AF Griffith, C. A. Penteado, P. Rannou, P. Brown, R. Boudon, V. Baines, K. H. Clark, R. Drossart, P. Buratti, B. Nicholson, P. McKay, C. P. Coustenis, A. Negrao, A. Jaumann, R. TI Evidence for a polar ethane cloud on Titan SO SCIENCE LA English DT Article ID SURFACE; ATMOSPHERE; METHANE; TEMPERATURES; TRITON; WINDS; RAIN; N-2; ICE AB Spectra from Cassini's Visual and Infrared Mapping Spectrometer reveal the presence of a vast tropospheric cloud on Titan at latitudes 51 degrees to 68 degrees north and all longitudes observed (10 degrees to 190 degrees west). The derived characteristics indicate that this cloud is composed of ethane and forms as a result of stratospheric subsidence and the particularly cool conditions near the moon's north pole. Preferential condensation of ethane, perhaps as ice, at Titan's poles during the winters may partially explain the lack of liquid ethane oceans on Titan's surface at middle and lower latitudes. C1 Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA. Univ Versailles, Serv Aeron, F-91371 Verrieres Le Buisson, France. Univ Bourgogne, Phys Lab, CNRS, UMR 5027, F-21078 Dijon, France. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. US Geol Survey, Denver, CO 80225 USA. Observ Paris, Meudon, France. Cornell Univ, Dept Astron, Ithaca, NY 14853 USA. NASA, Ames Res Ctr, Mountain View, CA USA. Observ Astron Lisboa, P-1349018 Lisbon, Portugal. Deutsch Zentrum Luft & Raumfahrt, Inst Planetary Explorat, Oberpfaffenhofen, Germany. RP Griffith, CA (reprint author), Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA. RI BOUDON, Vincent/A-4504-2010; Penteado, Paulo/F-9081-2012; RANNOU, Pascal/I-9059-2012; OI Penteado, Paulo/0000-0001-6759-2037; Negrao, Alberto/0000-0001-6042-1294 NR 34 TC 115 Z9 115 U1 1 U2 10 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 SEP 15 PY 2006 VL 313 IS 5793 BP 1620 EP 1622 DI 10.1126/science.1128245 PG 3 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 083YS UT WOS:000240498900040 PM 16973876 ER PT J AU Ferguson, FT Gardner, KG Nuth, JA AF Ferguson, Frank T. Gardner, Kathryn G. Nuth, Joseph A., III TI Vapor pressure of palladium from 1473 K to 1973 K SO JOURNAL OF CHEMICAL AND ENGINEERING DATA LA English DT Article ID THERMODYNAMIC PROPERTIES; MASS-SPECTROMETRY; VAPORIZATION; ALLOYS; METALS; OXIDE; IRON AB The vapor pressure of palladium was studied using a Knudsen effusion cell and a commercial thermogravimetric balance. Vapor pressures were measured using four Knudsen cells of different effusion areas with consistent results. Most of the available vapor pressure data for palladium has been taken below the fusion temperature, and only a few experimental studies exist on the vapor pressure of liquid palladium. In this current study, vapor pressures were measured from 1473 K to 1973 K ( from well above and well below the melting point). In addition, the range in temperature covered in the current study represents one of the largest continuous investigations of palladium vapor pressure to date. The standard enthalpy of sublimation calculated via a third-law analysis of the vapor pressure data is (377.7 +/- 0.2) kJ (.) mol(-1), in excellent agreement with the recommended value of (377 +/- 5) kJ (.) mol(-1) from the most recent review of available palladium vapor pressure data. C1 NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Catholic Univ Amer, Dept Chem, Washington, DC 20064 USA. Univ Oklahoma, Sch Geol & Geophys, Norman, OK 73019 USA. RP Ferguson, FT (reprint author), NASA, Goddard Space Flight Ctr, Code 691, Greenbelt, MD 20771 USA. EM frank.ferguson@gsfc.nasa.gov RI Ferguson, Frank/C-9493-2012; Nuth, Joseph/E-7085-2012 NR 28 TC 6 Z9 6 U1 1 U2 7 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 0021-9568 J9 J CHEM ENG DATA JI J. Chem. Eng. Data PD SEP 14 PY 2006 VL 51 IS 5 BP 1509 EP 1515 DI 10.1021/je050464i PG 7 WC Thermodynamics; Chemistry, Multidisciplinary; Engineering, Chemical SC Thermodynamics; Chemistry; Engineering GA 083YQ UT WOS:000240496200005 ER PT J AU Lieberman, RS Riggin, DM Garcia, RR Wu, Q Remsberg, EE AF Lieberman, R. S. Riggin, D. M. Garcia, R. R. Wu, Qian Remsberg, E. E. TI Observations of intermediate-scale diurnal waves in the equatorial mesosphere and lower thermosphere SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article ID COMMUNITY CLIMATE MODEL; QUASI-BIENNIAL OSCILLATION; TROPICAL MIDDLE ATMOSPHERE; GENERAL-CIRCULATION MODEL; SEMIANNUAL OSCILLATION; ZONAL WIND; GRAVITY-WAVES; SATELLITE-OBSERVATIONS; GEOPOTENTIAL HEIGHT; LIMS TEMPERATURES AB The purpose of this study is to seek observational evidence for diurnal, vertically propagating inertia-gravity waves (IGWs) in the mesosphere and lower thermosphere (MLT). Numerical modeling studies indicate that vertically propagating IGWs excited by tropical heating provide a significant source of momentum for the semiannual oscillation (SAO) in the equatorial zonal mean winds. The power spectrum of these waves has a strong diurnal component. We analyze global patterns of ascending and descending node differences in MLT satellite temperatures, which are assumed in this study to be proxies for waves of diurnal period. Juxtaposed upon the planetary-scale features are localized variations with longitudinal wavelengths ranging from 25 degrees to 50 degrees, and with vertical wavelengths between 13 and 25 km. These "intermediate-scale" variations are spatially coherent, and persist for several weeks. Their amplitudes generally increase with altitude, while their phase structures suggest both eastward and westward propagation. The variance of wave numbers 9-17 in the MLT is examined in relation to the underlying stratospheric zonal mean zonal gradient winds. Stronger variances generally coincide with periods where the underlying zonal mean winds are relatively light, or unidirectional. The weak inverse association between variance strength and zonal wind magnitude is suggestive of a wave filtering mechanism. C1 NW Res Associates, Colorado Res Associates Div, Boulder, CO 80301 USA. Natl Ctr Atmospher Res, Div Atmospher Chem, Boulder, CO 80305 USA. Natl Ctr Atmospher Res, High Altitude Observ, Boulder, CO 80307 USA. NASA, Langley Res Ctr, Hampton, VA 23681 USA. RP Lieberman, RS (reprint author), NW Res Associates, Colorado Res Associates Div, 3380 Mitchell Lane, Boulder, CO 80301 USA. EM ruth@cora.nwra.com NR 57 TC 2 Z9 2 U1 0 U2 0 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 SEP 14 PY 2006 VL 111 IS A10 AR A10S11 DI 10.1029/2005JA011498 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 086BN UT WOS:000240648200001 ER PT J AU Agarwal, GS Kapale, KT AF Agarwal, G. S. Kapale, K. T. TI Subwavelength atom localization via coherent population trapping SO JOURNAL OF PHYSICS B-ATOMIC MOLECULAR AND OPTICAL PHYSICS LA English DT Article ID PRECISION POSITION MEASUREMENT; MOVING ATOMS; OPTICAL-FIELDS; DIFFRACTION; INTERFERENCE; MOTION; LIGHT; LIMIT AB We present an atom localization scheme based on coherent population trapping. We consider atomic transitions in a Lambda configuration where the control field is a standing-wave field. The probe field and the control field produce coherence between the two ground states and prepare the atom in a pure state. We show that the population in one of the ground states has the same fringe pattern as produced by a Fabry-Perot interferometer and thus measurement of this population would localize the atom. Interestingly enough the role of the cavity finesse is played by the ratio of the intensities of the pump and probe. This is in fact the reason for obtaining extreme subwavelength localization. C1 Oklahoma State Univ, Dept Phys, Stillwater, OK 74078 USA. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. Louisiana State Univ, Dept Phys & Astron, Hearne Inst Theoret Phys, Baton Rouge, LA 70803 USA. RP Agarwal, GS (reprint author), Oklahoma State Univ, Dept Phys, Stillwater, OK 74078 USA. NR 24 TC 108 Z9 108 U1 0 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0953-4075 J9 J PHYS B-AT MOL OPT JI J. Phys. B-At. Mol. Opt. Phys. PD SEP 14 PY 2006 VL 39 IS 17 BP 3437 EP 3446 DI 10.1088/0953-4075/39/17/002 PG 10 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA 083XE UT WOS:000240490700005 ER PT J AU de Goncalves, LGG Shuttleworth, WJ Burke, EJ Houser, P Toll, DL Rodell, M Arsenault, K AF Gustavo Goncalves de Goncalves, L. Shuttleworth, William James Burke, Eleanor J. Houser, Paul Toll, David L. Rodell, Matthew Arsenault, Kristi TI Toward a South America Land Data Assimilation System: Aspects of land surface model spin-up using the simplified simple biosphere SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID SOIL-MOISTURE; PARAMETERIZATION SCHEMES; SNOW-PHYSICS; CLIMATE; IMPACT; WATER; CLASSIFICATION; PRECIPITATION; SIMULATIONS; CIRCULATION AB [1] This paper describes a spin-up experiment conducted over South America using the Simplified Simple Biosphere (SSiB) land surface model to study the process of model adjustment to atmospheric forcing data. The experiment was carried out as a precursor to the use of SSiB in a South American Land Data Assimilation System (SALDAS). The results from an 11 year long recursive simulation using three different initial conditions of soil wetness ( control, wet and dry) are examined. The control run was initiated by interpolation of the NCEP/DOE Global Reanalysis-2 (NCEP/DOE R- 2) soil moisture data set. In each case the time required for the model to reach equilibrium was calculated. The wet initialization leads to a faster adjustment of the soil moisture field, followed by the control and then the dry initialization. Overall, the final spin-up states using the SSiB-based SALDAS are generally wetter than both the NCEP/DOE R- 2 and the Centro de Previsao do Tempo e Estudos Climaticos (CPTEC - Brazilian Center for Weather Forecast and Climate Studies) operational initial soil moisture states, consequently modeled latent heat is higher and sensible heat lower in the final year of simulation when compared with the first year. Selected regions, i.e., in semiarid northeastern Brazil, the transition zone to the south of the Amazon tropical forest, and the central Andes were studied in more detail because they took longer to spin up ( up to 56 months) when compared with other areas ( less than 24 months). It is shown that there is a rapid change in the soil moisture in all layers in the first 2 months of simulation followed by a subsequent slow and steady adjustment: This could imply there are increasing errors in medium range simulations. Spin-up is longest where frozen soil is present for long periods such as in the central Andes. C1 Univ Arizona, Dept Hydrol & Water Resources, Tucson, AZ 85721 USA. Met Off Hadley Ctr Climate Predict & Res, Exeter EX1 3PB, Devon, England. Inst Global Environm & Soc, Ctr Res Environm & Water, Calverton, MD 20705 USA. George Mason Univ, Climate Dynam Program, Calverton, MD 20705 USA. NASA, Goddard Space Flight Ctr, Hydrol Sci Branch, Greenbelt, MD 20771 USA. RP de Goncalves, LGG (reprint author), NASA, Goddard Space Flight Ctr, Hydrol Sci Branch, Code 614-3, Greenbelt, MD 20771 USA. EM gustavo@hwr.arizona.edu RI Rodell, Matthew/E-4946-2012; Houser, Paul/J-9515-2013; OI Rodell, Matthew/0000-0003-0106-7437; Houser, Paul/0000-0002-2991-0441; de Goncalves, Luis Gustavo/0000-0002-1571-0916 NR 35 TC 13 Z9 13 U1 0 U2 0 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 SEP 13 PY 2006 VL 111 IS D17 AR D17110 DI 10.1029/2005JD006297 PG 13 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 085ZU UT WOS:000240643700001 ER PT J AU Haberle, RM Kahre, MA Murphy, JR Christensen, PR Greeley, R AF Haberle, R. M. Kahre, M. A. Murphy, J. R. Christensen, P. R. Greeley, R. TI Role of dust devils and orbital precession in closing the Martian dust cycle SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID GENERAL-CIRCULATION; MARS; SIMULATIONS; STORMS AB We use a general circulation model to simulate the role of dust devils on the Martian dust cycle as a function of orbital precession. We focus specifically on the two most recent epochs of 22,500 and 72,500 years ago when perihelion occurred near northern summer solstice. We find that dust devils dominate the dust cycle at these times and that while orbital precession does modulate the exchange of dust between the hemispheres, the integrated effect is a net transfer of dust from north to south. The low thermal inertia continents of Tharsis, Arabia, and Elysium are the main regions that contribute to the net loss in the Northern Hemisphere and this loss is primarily due to dust devils. These results suggests that the dust cycle is closed on time scales longer than those associated with orbital precession ( similar to 50,000 years) and that obliquity variations must also play an important role in the long-term dust cycle. C1 NASA, Ames Res Ctr, Space Sci & Astrobiol Div, Moffett Field, CA 94035 USA. New Mexico State Univ, Dept Astron, Las Cruces, NM 88003 USA. Arizona State Univ, Dept Geol Sci, Tempe, AZ 85287 USA. RP Haberle, RM (reprint author), NASA, Ames Res Ctr, Space Sci & Astrobiol Div, MS 245-3, Moffett Field, CA 94035 USA. EM robert.m.haberle@nasa.gov; kahrema@nmsu.edu; murphy@nmsu.edu; phil.christensen@asu.edu; greeley@asu.edu NR 16 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 EI 1944-8007 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD SEP 12 PY 2006 VL 33 IS 19 AR L19S04 DI 10.1029/2006GL026188 PG 4 WC Geosciences, Multidisciplinary SC Geology GA 085ZQ UT WOS:000240643300001 ER PT J AU MacAyeal, DR Okal, EA Aster, RC Bassis, JN Brunt, KM Cathles, LM Drucker, R Fricker, HA Kim, YJ Martin, S Okal, MH Sergienko, OV Sponsler, MP Thom, JE AF MacAyeal, Douglas R. Okal, Emile A. Aster, Richard C. Bassis, Jeremy N. Brunt, Kelly M. Cathles, L. Mac. Drucker, Robert Fricker, Helen A. Kim, Young-Jin Martin, Seelye Okal, Marianne H. Sergienko, Olga V. Sponsler, Mark P. Thom, Jonathan E. TI Transoceanic wave propagation links iceberg calving margins of Antarctica with storms in tropics and Northern Hemisphere SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID ICE-SHELF; ATLANTIC; SWELL; SEA AB We deployed seismometers on the Ross Ice Shelf and on various icebergs adrift in the Ross Sea ( including B15A, a large 100 km by 30 km fragment of B15, which calved from the Ross Ice Shelf in March, 2000). The data reveal that the dominant energy of these floating ice masses is in the 0.01 to 0.1 Hz band, and is associated with sea swell generated in the tropical and extra-tropical Pacific Ocean. In one example, a strong storm in the Gulf of Alaska on 21 October 2005, approximately 13,500 km from the Ross Sea, generated swell that arrived at B15A immediately prior to, and during, its break-up off Cape Adare on 27 October 2005. If sea swell influences iceberg calving and break-up, a teleconnection exists between the Antarctic ice sheet mass balance and weather systems worldwide. C1 Univ Chicago, Dept Geophys Sci, Chicago, IL 60637 USA. Northwestern Univ, Dept Geol Sci, Evanston, IL 60208 USA. New Mexico Inst Min & Technol, Geophys Res Ctr, Socorro, NM 87801 USA. New Mexico Inst Min & Technol, Dept Earth & Environm Sci, Socorro, NM 87801 USA. Univ Calif San Diego, Scripps Inst Oceanog, Inst Geophys & Planetary Phys, La Jolla, CA 92093 USA. Univ Washington, Sch Oceanog, Seattle, WA 98195 USA. Stormsurf, Half Moon Bay, CA 94019 USA. Univ Wisconsin, Antarctic Meteorol Res Ctr, Madison, WI 54025 USA. NASA, Goddard Space Flight Ctr, Hydrospher & Biospher Sci Lab, Greenbelt, MD 20771 USA. RP MacAyeal, DR (reprint author), Univ Chicago, Dept Geophys Sci, 5734 S Ellis Ave, Chicago, IL 60637 USA. EM drm7@midway.uchicago.edu RI Bassis, Jeremy/J-1706-2012; OI Bassis, Jeremy/0000-0003-2946-7176; MacAyeal, Douglas/0000-0003-0647-6176; Okal, Marianne/0000-0002-9344-6196 NR 20 TC 46 Z9 46 U1 1 U2 3 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 EI 1944-8007 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD SEP 12 PY 2006 VL 33 IS 17 AR L17502 DI 10.1029/2006GL027235 PG 4 WC Geosciences, Multidisciplinary SC Geology GA 085ZE UT WOS:000240642100009 ER PT J AU Xu, JY She, CY Yuan, W Mertens, C Mlynczak, M Russell, J AF Xu, Jiyao She, C. Y. Yuan, Wei Mertens, Chris Mlynczak, Marty Russell, James TI Comparison between the temperature measurements by TIMED/SABER and lidar in the midlatitude SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article ID MESOSPHERIC WATER-VAPOR; NON-LTE CONDITIONS; MIDDLE ATMOSPHERE; MESOPAUSE REGION; ATOMIC OXYGEN; FORT-COLLINS; LOWER THERMOSPHERE; THERMAL STRUCTURE; MU-M; 40-DEGREES-N LATITUDE AB Comparisons of monthly mean nighttime temperature profiles observed by the sodium lidar at Colorado State University and TIMED/SABER overpasses are made. In the altitude range from 85 km to about 100 km, the two observations are in very good agreement. Though within each other's error bars, important differences occur below 85 km in the entire year and above 100 km in the summer season. Possible reasons for these difference are high photon noise below 85 km in lidar observations and less than accurate assumptions in the concentration of important chemical species like oxygen (and its quenching rate) in the SABER retrieval above 100 km. However, the two techniques both show the two-level mesopause thermal structure, with the times of change from one level to the other in excellent agreement. Comparison indicates that the high-level (winter) mesopause altitudes are also in excellent agreement between the two observations, though some difference (2-3 km) may exist in the low-level (summer) mesopause altitudes between ground- based and satellite-borne data. In addition, the difference in local time dependency between lidar and SABER is investigated; this difference makes the comparison of mesopause altitudes difficult. C1 Chinese Acad Sci, Ctr Space Sci & Appl Res, Key Lab Space Weather, Beijing 100080, Peoples R China. Colorado State Univ, Dept Phys, Ft Collins, CO 80523 USA. NASA, Langley Res Ctr, Hampton, VA 23681 USA. Hampton Univ, Ctr Atmospher Sci, Hampton, VA 23668 USA. RP Xu, JY (reprint author), Chinese Acad Sci, Ctr Space Sci & Appl Res, Key Lab Space Weather, POB 8701, Beijing 100080, Peoples R China. EM joeshe@lamar.colostate.edu RI Mlynczak, Martin/K-3396-2012 NR 36 TC 21 Z9 21 U1 2 U2 9 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0148-0227 J9 J GEOPHYS RES-SPACE JI J. Geophys. Res-Space Phys. PD SEP 12 PY 2006 VL 111 IS A10 AR A10S09 DI 10.1029/2005JA011439 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 086BL UT WOS:000240648000001 ER PT J AU Vander Wal, RL AF Vander Wal, Randall L. TI Synthesis and applications or inorganic and organic nanomaterials SO ABSTRACTS OF PAPERS OF THE AMERICAN CHEMICAL SOCIETY LA English DT Meeting Abstract C1 [Vander Wal, Randall L.] NASA, NCSER, Glenn Res Ctr, Cleveland, OH 44135 USA. NR 0 TC 0 Z9 0 U1 0 U2 1 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 0065-7727 J9 ABSTR PAP AM CHEM S JI Abstr. Pap. Am. Chem. Soc. PD SEP 10 PY 2006 VL 232 MA 33-AEI BP 81 EP 81 PG 1 WC Chemistry, Multidisciplinary SC Chemistry GA V15DB UT WOS:000207781600077 ER PT J AU Wilson, EW Hamilton, WA Mount, HR DeMore, WB AF Wilson, Edmond W., Jr. Hamilton, Wesley A. Mount, Hillary R. DeMore, William B. TI Rate constants for the reactions of hydroxyl radical with several fluoroethers by the relative rate method SO ABSTRACTS OF PAPERS OF THE AMERICAN CHEMICAL SOCIETY LA English DT Meeting Abstract C1 [Wilson, Edmond W., Jr.; Hamilton, Wesley A.; Mount, Hillary R.] Harding Univ, Dept Phys Sci, Searcy, AR 72149 USA. [DeMore, William B.] Jet Prop Lab, Fallbrook, CA 92028 USA. NR 0 TC 0 Z9 0 U1 0 U2 1 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 0065-7727 J9 ABSTR PAP AM CHEM S JI Abstr. Pap. Am. Chem. Soc. PD SEP 10 PY 2006 VL 232 MA 203-ENVR BP 733 EP 733 PG 1 WC Chemistry, Multidisciplinary SC Chemistry GA V15DB UT WOS:000207781604664 ER PT J AU Holladay, J Brooks, KP Humble, PH Lilley, BP Hu, JL Simon, T AF Holladay, Jamie Brooks, Kriston P. Humble, Paul H. Lilley, Brian P. Hu, Jianli Simon, Thomas TI Rocket propellant production on Mars using microchannel technology SO ABSTRACTS OF PAPERS OF THE AMERICAN CHEMICAL SOCIETY LA English DT Meeting Abstract C1 [Holladay, Jamie; Brooks, Kriston P.; Humble, Paul H.; Lilley, Brian P.] Pacific NW Div, Richland, WA 99352 USA. [Hu, Jianli] Pacific NW Natl Lab, Richland, WA 99352 USA. [Simon, Thomas] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. RI Humble, Paul/K-1961-2012; Humble, Paul/E-4766-2015 OI Humble, Paul/0000-0002-2632-6557; NR 0 TC 0 Z9 0 U1 0 U2 1 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 0065-7727 J9 ABSTR PAP AM CHEM S JI Abstr. Pap. Am. Chem. Soc. PD SEP 10 PY 2006 VL 232 MA 139-IEC BP 817 EP 817 PG 1 WC Chemistry, Multidisciplinary SC Chemistry GA V15DB UT WOS:000207781604705 ER PT J AU Miller, S Heimann, P Scheiman, DA AF Miller, Sandi Heimann, Paula Scheiman, Daniel A. TI Effect of graphite surface modification on the properties of exfoliated graphene oxide/epoxy nanocomposites SO ABSTRACTS OF PAPERS OF THE AMERICAN CHEMICAL SOCIETY LA English DT Meeting Abstract C1 [Miller, Sandi] NASA, Polymer Mat Branch, Cleveland, OH 44135 USA. [Heimann, Paula] NASA Glenn Res Ctr, Ohio Aerosp Inst, Cleveland, OH 44135 USA. [Scheiman, Daniel A.] NASA Glenn, QSS Grp Inc, Cleveland, OH 44135 USA. NR 0 TC 0 Z9 0 U1 2 U2 8 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 0065-7727 J9 ABSTR PAP AM CHEM S JI Abstr. Pap. Am. Chem. Soc. PD SEP 10 PY 2006 VL 232 MA 12-IEC BP 960 EP 960 PG 1 WC Chemistry, Multidisciplinary SC Chemistry GA V15DB UT WOS:000207781604848 ER PT J AU Anderson, MS AF Anderson, Mark S. TI ANYL 9-Shear driven nano-chromatography SO ABSTRACTS OF PAPERS OF THE AMERICAN CHEMICAL SOCIETY LA English DT Meeting Abstract C1 [Anderson, Mark S.] CALTECH, Jet Prop Lab, Analyt Chem & Mat Dev Grp, Pasadena, CA 91109 USA. NR 0 TC 0 Z9 0 U1 1 U2 3 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 0065-7727 J9 ABSTR PAP AM CHEM S JI Abstr. Pap. Am. Chem. Soc. PD SEP 10 PY 2006 VL 232 MA 9-ANYL PG 1 WC Chemistry, Multidisciplinary SC Chemistry GA V15DB UT WOS:000207781601198 ER PT J AU Boxe, CS AF Boxe, Christopher S. TI COLL 132-Kinetics of NO and NO2 evolution from illuminated frozen nitrate solutions SO ABSTRACTS OF PAPERS OF THE AMERICAN CHEMICAL SOCIETY LA English DT Meeting Abstract C1 [Boxe, Christopher S.] NASA JPL, Earth & Space Sci Div, Lab Studies & Modeling, Pasadena, CA 91109 USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 0065-7727 J9 ABSTR PAP AM CHEM S JI Abstr. Pap. Am. Chem. Soc. PD SEP 10 PY 2006 VL 232 MA 132-COLL PG 1 WC Chemistry, Multidisciplinary SC Chemistry GA V15DB UT WOS:000207781603716 ER PT J AU Brown, SR Kauzlarich, SM Gascoin, F Snyder, GJ AF Brown, Shawna R. Kauzlarich, Susan M. Gascoin, Franck Snyder, G. Jeffrey TI INOR 915-Improving thermoelectric figure of merit: Investigation of Zn-doped Yb14MnSb11 SO ABSTRACTS OF PAPERS OF THE AMERICAN CHEMICAL SOCIETY LA English DT Meeting Abstract C1 [Brown, Shawna R.; Kauzlarich, Susan M.] Univ Calif Davis, Dept Chem, Davis, CA 95616 USA. [Gascoin, Franck; Snyder, G. Jeffrey] Calif Tech Inst, Jet Prop Lab, Pasadena, CA 91109 USA. RI Snyder, G/I-2263-2015 NR 0 TC 0 Z9 0 U1 0 U2 1 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 0065-7727 J9 ABSTR PAP AM CHEM S JI Abstr. Pap. Am. Chem. Soc. PD SEP 10 PY 2006 VL 232 MA 915-INOR PG 1 WC Chemistry, Multidisciplinary SC Chemistry GA V15DB UT WOS:000207781607803 ER PT J AU Cable, ML Kirby, JP Sorasaenee, K Gray, HB Ponce, A AF Cable, Morgan L. Kirby, James P. Sorasaenee, Karn Gray, Harry B. Ponce, Adrian TI INOR 209-Characterization of a lanthanide sensor molecule for bacterial spore detection SO ABSTRACTS OF PAPERS OF THE AMERICAN CHEMICAL SOCIETY LA English DT Meeting Abstract C1 [Cable, Morgan L.; Gray, Harry B.] CALTECH, Beckman Inst, Pasadena, CA 91125 USA. [Kirby, James P.; Ponce, Adrian] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Sorasaenee, Karn] CALTECH, Div Chem & Chem Engn, Pasadena, CA 91125 USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 0065-7727 J9 ABSTR PAP AM CHEM S JI Abstr. Pap. Am. Chem. Soc. PD SEP 10 PY 2006 VL 232 MA 209-INOR PG 1 WC Chemistry, Multidisciplinary SC Chemistry GA V15DB UT WOS:000207781606223 ER PT J AU Cable, ML Kirby, JP Sorasaenee, K Gray, HB Ponce, A AF Cable, Morgan L. Kirby, James P. Sorasaenee, Karn Gray, Harry B. Ponce, Adrian TI INOR 970-Terbium macrocycle dipicolinate receptor site for bacterial spore detection SO ABSTRACTS OF PAPERS OF THE AMERICAN CHEMICAL SOCIETY LA English DT Meeting Abstract C1 [Cable, Morgan L.; Gray, Harry B.] CALTECH, Beckman Inst, Pasadena, CA 91125 USA. [Kirby, James P.; Ponce, Adrian] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Sorasaenee, Karn] CALTECH, Div Chem & Chem Engn, Pasadena, CA 91125 USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 0065-7727 J9 ABSTR PAP AM CHEM S JI Abstr. Pap. Am. Chem. Soc. PD SEP 10 PY 2006 VL 232 MA 970-INOR PG 1 WC Chemistry, Multidisciplinary SC Chemistry GA V15DB UT WOS:000207781606222 ER PT J AU Chung, HY Levine, J Weinberger, M Blair, R Rasool, H Tolbert, S Yang, JM Kaner, RB AF Chung, H. Y. Levine, J. Weinberger, M. Blair, R. Rasool, H. Tolbert, S. Yang, J-M. Kaner, R. B. TI INOR 811-Rhenium diboride, an ultra-incompressible, hard material SO ABSTRACTS OF PAPERS OF THE AMERICAN CHEMICAL SOCIETY LA English DT Meeting Abstract C1 [Chung, H. Y.; Yang, J-M.] Univ Calif Los Angeles, Dept Mat Sci & Engn, Los Angeles, CA 90095 USA. [Levine, J.; Weinberger, M.; Rasool, H.; Tolbert, S.; Kaner, R. B.] Univ Calif Los Angeles, Dept Chem & Biochem, Los Angeles, CA 90095 USA. [Blair, R.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RI Tolbert, Sarah/L-2321-2016 NR 0 TC 0 Z9 0 U1 0 U2 0 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 0065-7727 J9 ABSTR PAP AM CHEM S JI Abstr. Pap. Am. Chem. Soc. PD SEP 10 PY 2006 VL 232 MA 811-INOR PG 1 WC Chemistry, Multidisciplinary SC Chemistry GA V15DB UT WOS:000207781606939 ER PT J AU Crochet, AP Francis, MB Paavola, C AF Crochet, Amanda P. Francis, Matthew B. Paavola, Chad TI ORGN 756-Periplasmic binding proteins as biosensors: A synthetic approach SO ABSTRACTS OF PAPERS OF THE AMERICAN CHEMICAL SOCIETY LA English DT Meeting Abstract C1 [Crochet, Amanda P.; Francis, Matthew B.] Univ Calif Berkeley, Dept Chem, Berkeley, CA 94720 USA. [Paavola, Chad] NASA Ames Res Ctr, Ctr Nanotechnol, Mountain View, CA 94305 USA. [Paavola, Chad] NASA Ames Res Ctr, Astrobiol Technol Branch, Mountain View, CA 94305 USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 0065-7727 J9 ABSTR PAP AM CHEM S JI Abstr. Pap. Am. Chem. Soc. PD SEP 10 PY 2006 VL 232 MA 756-ORGN PG 1 WC Chemistry, Multidisciplinary SC Chemistry GA V15DB UT WOS:000207781608449 ER PT J AU Gorelik, O Sosa, E Nikolaev, P Holmes, W Arepalli, S Yowell, L AF Gorelik, Olga Sosa, Ed Nikolaev, Pavel Holmes, William Arepalli, Sivaram Yowell, Leonard TI PRES 47-Large-scale purification of laser and HiPco carbon nanotubes by soft-baking SO ABSTRACTS OF PAPERS OF THE AMERICAN CHEMICAL SOCIETY LA English DT Meeting Abstract C1 [Gorelik, Olga; Sosa, Ed; Nikolaev, Pavel; Holmes, William; Arepalli, Sivaram] ERC Inc NASA JSC, Houston, TX 77258 USA. [Yowell, Leonard] NASA JSC, Houston, TX 77258 USA. NR 2 TC 0 Z9 0 U1 0 U2 1 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 0065-7727 J9 ABSTR PAP AM CHEM S JI Abstr. Pap. Am. Chem. Soc. PD SEP 10 PY 2006 VL 232 MA 47-PRES PG 1 WC Chemistry, Multidisciplinary SC Chemistry GA V15DB UT WOS:000207781605746 ER PT J AU Huang, XC Carter, S Bowman, JM AF Huang, Xinchuan Carter, Stuart Bowman, Joel M. TI PHYS 445-Quantum simulations of water dimer IR spectra SO ABSTRACTS OF PAPERS OF THE AMERICAN CHEMICAL SOCIETY LA English DT Meeting Abstract C1 [Huang, Xinchuan] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Carter, Stuart; Bowman, Joel M.] Emory Univ, Dept Chem, Atlanta, GA 30322 USA. [Carter, Stuart; Bowman, Joel M.] Emory Univ, Cherry L Emerson Ctr Sci Computat, Atlanta, GA 30322 USA. RI HUANG, XINCHUAN/A-3266-2013 NR 1 TC 0 Z9 0 U1 0 U2 1 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 0065-7727 J9 ABSTR PAP AM CHEM S JI Abstr. Pap. Am. Chem. Soc. PD SEP 10 PY 2006 VL 232 MA 445-PHYS PG 1 WC Chemistry, Multidisciplinary SC Chemistry GA V15DB UT WOS:000207781609135 ER PT J AU Jaffe, C Ross, SD Lo, MW Marsden, J Farrelly, D Uzer, T AF Jaffe, Charles Ross, Shane D. Lo, Martin W. Marsden, Jerrold Farrelly, David Uzer, Turgay TI PHYS 258-Statistical theory of asteroid escape rates SO ABSTRACTS OF PAPERS OF THE AMERICAN CHEMICAL SOCIETY LA English DT Meeting Abstract C1 [Ross, Shane D.; Marsden, Jerrold] CALTECH, Control & Dynam Syst Div 107 81, Pasadena, CA 91125 USA. [Jaffe, Charles] W Virginia Univ, Dept Chem, Morgantown, WV 26505 USA. [Lo, Martin W.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Farrelly, David] Utah State Univ, Dept Chem, Logan, UT 84322 USA. [Uzer, Turgay] Georgia Inst Technol, Sch Phys, Ctr Nonlinear Sci, Atlanta, GA 30332 USA. RI Ross, Shane/B-7237-2009 OI Ross, Shane/0000-0001-5523-2376 NR 0 TC 0 Z9 0 U1 0 U2 0 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 0065-7727 J9 ABSTR PAP AM CHEM S JI Abstr. Pap. Am. Chem. Soc. PD SEP 10 PY 2006 VL 232 MA 258-PHYS PG 1 WC Chemistry, Multidisciplinary SC Chemistry GA V15DB UT WOS:000207781609307 ER PT J AU Jaffe, RL Philpott, MR Kawazoe, Y AF Jaffe, R. L. Philpott, M. R. Kawazoe, Y. TI INOR 1042-Hydrogenation of dinitrogen starting from a Zirconocene-N2 adduct: Calculation of pathways for NH3 synthesis SO ABSTRACTS OF PAPERS OF THE AMERICAN CHEMICAL SOCIETY LA English DT Meeting Abstract C1 [Jaffe, R. L.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Philpott, M. R.; Kawazoe, Y.] Tohuku Univ, Inst Mat Res, Sendai, Miyagi 9808577, Japan. NR 0 TC 0 Z9 0 U1 0 U2 0 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 0065-7727 J9 ABSTR PAP AM CHEM S JI Abstr. Pap. Am. Chem. Soc. PD SEP 10 PY 2006 VL 232 MA 1042-INOR PG 1 WC Chemistry, Multidisciplinary SC Chemistry GA V15DB UT WOS:000207781606411 ER PT J AU Kojiro, DR Lee, GS AF Kojiro, Daniel R. Lee, Geoffrey S. TI SCHB 14-A tale of two small business grants: The best of times, the worst of times from the NASA Ames Small Business Innovative Research (SBIR) Program SO ABSTRACTS OF PAPERS OF THE AMERICAN CHEMICAL SOCIETY LA English DT Meeting Abstract C1 [Kojiro, Daniel R.] NASA, Space Sci & Astrobiol Div, Ames Res Ctr, Exobiol Branch, Moffett Field, CA 94035 USA. [Lee, Geoffrey S.] NASA, Small Business Innovat Res Program, Ames Res Ctr, Moffett Field, CA 94035 USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 0065-7727 J9 ABSTR PAP AM CHEM S JI Abstr. Pap. Am. Chem. Soc. PD SEP 10 PY 2006 VL 232 MA 14-SCHB PG 1 WC Chemistry, Multidisciplinary SC Chemistry GA V15DB UT WOS:000207781603814 ER PT J AU Lebron-Colon, M Meador, MA AF Lebron-Colon, Marisabel Meador, Michael A. TI INOR 752-Photo-oxidation of single-wall carbon nanotubes SO ABSTRACTS OF PAPERS OF THE AMERICAN CHEMICAL SOCIETY LA English DT Meeting Abstract C1 [Lebron-Colon, Marisabel; Meador, Michael A.] NASA, Mat & Struct Div, Glenn Res Ctr, Cleveland, OH 44135 USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 0065-7727 J9 ABSTR PAP AM CHEM S JI Abstr. Pap. Am. Chem. Soc. PD SEP 10 PY 2006 VL 232 MA 752-INOR PG 1 WC Chemistry, Multidisciplinary SC Chemistry GA V15DB UT WOS:000207781606807 ER PT J AU Lenihan, JS Ball, JC Gayalas, VG Lumpp, JK Hines, J Daunert, S Bachas, LG AF Lenihan, Jeffrey S. Ball, J. Christopher Gayalas, Vasilis G. Lumpp, Janet K. Hines, John Daunert, Sylvia Bachas, Leonidas G. TI ANYL 118-Ion-selective sensing in micromachined electrochemical cells with nanoliter-range volume SO ABSTRACTS OF PAPERS OF THE AMERICAN CHEMICAL SOCIETY LA English DT Meeting Abstract C1 [Lenihan, Jeffrey S.; Gayalas, Vasilis G.; Daunert, Sylvia; Bachas, Leonidas G.] Univ Kentucky, Dept Chem, Lexington, KY 40506 USA. [Ball, J. Christopher] American Univ, Washington, DC 20016 USA. [Lumpp, Janet K.] Univ Kentucky, Dept Elect Engn, Lexington, KY 40506 USA. [Hines, John] NASA, Ames Res Ctr, Washington, DC USA. RI Bachas, Leonidas/G-2479-2015 NR 0 TC 0 Z9 0 U1 0 U2 0 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 0065-7727 J9 ABSTR PAP AM CHEM S JI Abstr. Pap. Am. Chem. Soc. PD SEP 10 PY 2006 VL 232 MA 118-ANYL PG 1 WC Chemistry, Multidisciplinary SC Chemistry GA V15DB UT WOS:000207781601003 ER PT J AU Nikolaev, P Arepalli, S Sosa, E Gorelik, O Holmes, W Moloney, P Allada, RK Waid, M Yowell, L AF Nikolaev, Pavel Arepalli, Sivaram Sosa, Ed Gorelik, Olga Holmes, William Moloney, Padraig Allada, Ram Kumar Waid, Michael Yowell, Leonard TI PRES 34-Carbon nanomaterials for human spaceflight applications SO ABSTRACTS OF PAPERS OF THE AMERICAN CHEMICAL SOCIETY LA English DT Meeting Abstract C1 [Nikolaev, Pavel; Arepalli, Sivaram; Sosa, Ed; Gorelik, Olga; Holmes, William] ERC Inc NASA JSC, Houston, TX 77258 USA. [Moloney, Padraig; Allada, Ram Kumar; Waid, Michael; Yowell, Leonard] NASA JSC, Houston, TX 77258 USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 0065-7727 J9 ABSTR PAP AM CHEM S JI Abstr. Pap. Am. Chem. Soc. PD SEP 10 PY 2006 VL 232 MA 34-PRES PG 1 WC Chemistry, Multidisciplinary SC Chemistry GA V15DB UT WOS:000207781605740 ER PT J AU Okumura, M Mollner, AK Fry, JL Sander, SP Roehl, CM Wennberg, PO McCoy, AB Francisco, JS AF Okumura, Mitchio Mollner, Andrew K. Fry, Juliane L. Sander, Stanley P. Roehl, Coleen M. Wennberg, Paul O. McCoy, Anne B. Francisco, Joseph S. TI PHYS 130-The termolecular association reaction OH+NO2+M SO ABSTRACTS OF PAPERS OF THE AMERICAN CHEMICAL SOCIETY LA English DT Meeting Abstract C1 [Okumura, Mitchio; Mollner, Andrew K.; Fry, Juliane L.] CALTECH, Div Chem & Chem Engn, Arthur Amos Noyes Lab Chem Phys, Pasadena, CA 91125 USA. [Sander, Stanley P.] CALTECH, Jet Prop Lab, Div Earth & Space Sci, Pasadena, CA 91109 USA. [Roehl, Coleen M.; Wennberg, Paul O.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. [McCoy, Anne B.] Ohio State Univ, Dept Chem, Columbus, OH 43210 USA. [Francisco, Joseph S.] Purdue Univ, Dept Chem, W Lafayette, IN 47907 USA. RI Wennberg, Paul/A-5460-2012 NR 0 TC 0 Z9 0 U1 0 U2 1 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 0065-7727 J9 ABSTR PAP AM CHEM S JI Abstr. Pap. Am. Chem. Soc. PD SEP 10 PY 2006 VL 232 MA 130-PHYS PG 1 WC Chemistry, Multidisciplinary SC Chemistry GA V15DB UT WOS:000207781609346 ER PT J AU Philpott, MR Jaffe, RL Kawazoe, Y AF Philpott, Michael R. Jaffe, R. L. Kawazoe, Yoshiyuki TI INOR 902-Ab initio electronic structure-property-function calculations of Fe8S9(SH)2 as a model for nitrogenase cofactor SO ABSTRACTS OF PAPERS OF THE AMERICAN CHEMICAL SOCIETY LA English DT Meeting Abstract C1 [Philpott, Michael R.] Tohoku Univ, Ctr Computat Mat Sci, Inst Mat Res, Aoba Ku, Sendai, Miyagi 9808577, Japan. [Jaffe, R. L.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. NR 0 TC 0 Z9 0 U1 1 U2 1 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 0065-7727 J9 ABSTR PAP AM CHEM S JI Abstr. Pap. Am. Chem. Soc. PD SEP 10 PY 2006 VL 232 MA 902-INOR PG 1 WC Chemistry, Multidisciplinary SC Chemistry GA V15DB UT WOS:000207781607769 ER PT J AU Prokopuk, N Son, KA Waltz, C AF Prokopuk, Nicholas Son, Kyung-ah Waltz, Chad TI INOR 596-Nanocrossbar structures for probing electron tunneling through fluid solvents SO ABSTRACTS OF PAPERS OF THE AMERICAN CHEMICAL SOCIETY LA English DT Meeting Abstract C1 [Prokopuk, Nicholas; Waltz, Chad] USN, Chem & Mat Div, Air Warfare Ctr, China Lake, CA 93555 USA. [Son, Kyung-ah] CALTECH, Jet Prop Lab, Nano & Micro Syst Grp, Pasadena, CA 91109 USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 0065-7727 J9 ABSTR PAP AM CHEM S JI Abstr. Pap. Am. Chem. Soc. PD SEP 10 PY 2006 VL 232 MA 596-INOR PG 1 WC Chemistry, Multidisciplinary SC Chemistry GA V15DB UT WOS:000207781606332 ER PT J AU Pun, TY Shafaat, HS Connon, SA Ponce, A AF Pun To Yung Shafaat, Hannah S. Connon, Stephanie A. Ponce, Adrian TI INOR 256-Quantification of bacterial spores capable of germination in GISP2 ice cores using a novel endospore viability assay SO ABSTRACTS OF PAPERS OF THE AMERICAN CHEMICAL SOCIETY LA English DT Meeting Abstract C1 [Pun To Yung; Shafaat, Hannah S.; Connon, Stephanie A.; Ponce, Adrian] Jet Prop Lab, Pasadena, CA 91109 USA. RI Connon, Stephanie/K-1959-2012 NR 0 TC 0 Z9 0 U1 0 U2 0 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 0065-7727 J9 ABSTR PAP AM CHEM S JI Abstr. Pap. Am. Chem. Soc. PD SEP 10 PY 2006 VL 232 MA 256-INOR PG 1 WC Chemistry, Multidisciplinary SC Chemistry GA V15DB UT WOS:000207781606785 ER PT J AU Rhee, YM Lee, T Allamandola, LJ Gudipati, MS Head-Gordon, M AF Rhee, Young M. Lee, Timothy Allamandola, Louis J. Gudipati, Murthy S. Head-Gordon, Martin TI PHYS 684-Stable dimeric bond formation in polycyclic aromatic hydrocarbons: Quantum chemical assessment SO ABSTRACTS OF PAPERS OF THE AMERICAN CHEMICAL SOCIETY LA English DT Meeting Abstract C1 [Rhee, Young M.; Head-Gordon, Martin] Univ Calif Berkeley, Dept Chem, Berkeley, CA 94720 USA. [Lee, Timothy; Allamandola, Louis J.; Gudipati, Murthy S.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Head-Gordon, Martin] Univ Calif Berkeley, Lawrence Berkeley Lab, Div Chem Sci, Berkeley, CA 94720 USA. RI Gudipati, Murthy/F-7575-2011 NR 0 TC 0 Z9 0 U1 1 U2 2 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 0065-7727 J9 ABSTR PAP AM CHEM S JI Abstr. Pap. Am. Chem. Soc. PD SEP 10 PY 2006 VL 232 MA 684-PHYS PG 1 WC Chemistry, Multidisciplinary SC Chemistry GA V15DB UT WOS:000207781609464 ER PT J AU Sosa, E Nikolaev, P Holmes, W Gorelik, O Arepalli, S Yowell, L AF Sosa, Ed Nikolaev, Pavel Holmes, William Gorelik, Olga Arepalli, Sivaram Yowell, Leonard TI PRES 60-Variability of single wall carbon nanotubes produced by pulsed laser vaporization, arc discharge and HiPco SO ABSTRACTS OF PAPERS OF THE AMERICAN CHEMICAL SOCIETY LA English DT Meeting Abstract C1 [Sosa, Ed; Nikolaev, Pavel; Holmes, William; Gorelik, Olga; Arepalli, Sivaram] ERC Inc NASA JSC, Houston, TX 77258 USA. [Yowell, Leonard] NASA JSC, Houston, TX 77258 USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 0065-7727 J9 ABSTR PAP AM CHEM S JI Abstr. Pap. Am. Chem. Soc. PD SEP 10 PY 2006 VL 232 MA 60-PRES PG 1 WC Chemistry, Multidisciplinary SC Chemistry GA V15DB UT WOS:000207781605742 ER PT J AU Vander Wal, RL Hays, MD AF Vander Wal, Randall L. Hays, Michael D. TI ANYL 341-Carbon nanostructure characterization by XPS SO ABSTRACTS OF PAPERS OF THE AMERICAN CHEMICAL SOCIETY LA English DT Meeting Abstract C1 [Vander Wal, Randall L.] NASA, Glenn Res Ctr, NCSER, Cleveland, OH 44135 USA. [Hays, Michael D.] US EPA, Natl Risk Management Res Lab, Res Triangle Pk, NC 27711 USA. NR 0 TC 0 Z9 0 U1 0 U2 1 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 0065-7727 J9 ABSTR PAP AM CHEM S JI Abstr. Pap. Am. Chem. Soc. PD SEP 10 PY 2006 VL 232 MA 341-ANYL PG 1 WC Chemistry, Multidisciplinary SC Chemistry GA V15DB UT WOS:000207781601157 ER PT J AU Xu, JC Hunter, GW Liu, CC Ward, B Artale, M Lampard, P Androjna, D AF Xu, Jennifer C. Hunter, Gary W. Liu, Chung-Chiun Ward, Benjamin Artale, Michael Lampard, Peter Androjna, Drago TI INOR 476-Miniature amperometric solid electrolyte oxygen sensor SO ABSTRACTS OF PAPERS OF THE AMERICAN CHEMICAL SOCIETY LA English DT Meeting Abstract C1 [Xu, Jennifer C.; Hunter, Gary W.] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. [Liu, Chung-Chiun] Case Western Reserve Univ, Cleveland, OH 44106 USA. [Ward, Benjamin] Makel Engn, Chico, CA 95973 USA. [Artale, Michael; Lampard, Peter; Androjna, Drago] Sierra Lobo, Clevalnd, OH 44135 USA. NR 0 TC 0 Z9 0 U1 1 U2 2 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 0065-7727 J9 ABSTR PAP AM CHEM S JI Abstr. Pap. Am. Chem. Soc. PD SEP 10 PY 2006 VL 232 MA 476-INOR PG 1 WC Chemistry, Multidisciplinary SC Chemistry GA V15DB UT WOS:000207781606857 ER PT J AU Yung, PT Shafaat, HS Connon, SA Yang, WW Lester, ED Ponce, A AF Yung, Pun To Shafaat, Hannah S. Connon, Stephanie A. Yang, Wanwan Lester, Elizabeth D. Ponce, Adrian TI PHYS 486-Survival of bacterial spores in extreme environments: Validation and application of a novel endospore viability assay SO ABSTRACTS OF PAPERS OF THE AMERICAN CHEMICAL SOCIETY LA English DT Meeting Abstract C1 [Yung, Pun To; Shafaat, Hannah S.; Connon, Stephanie A.; Yang, Wanwan; Lester, Elizabeth D.; Ponce, Adrian] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RI Connon, Stephanie/K-1959-2012 NR 0 TC 0 Z9 0 U1 0 U2 1 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 0065-7727 J9 ABSTR PAP AM CHEM S JI Abstr. Pap. Am. Chem. Soc. PD SEP 10 PY 2006 VL 232 MA 486-PHYS PG 1 WC Chemistry, Multidisciplinary SC Chemistry GA V15DB UT WOS:000207781609375 ER PT J AU Veselovskii, I Korenskii, M Griaznov, V Whiteman, DN McGill, M Roy, G Bissonnette, L AF Veselovskii, Igor Korenskii, Michail Griaznov, Vadim Whiteman, David N. McGill, Matthew Roy, Gilles Bissonnette, Luc TI Information content of data measured with a multiple-field-of-view lidar SO APPLIED OPTICS LA English DT Article ID RETURNS; CLOUDS AB Lidars with multiple fields of view (MFOVs) are promising tools for gaining information on cloud particle size. We perform a study of the information content of MFOV lidar data with the use of eigenvalue analysis. The approach we have developed permits an understanding of the main features of MFOV lidars and provides a way to relate the accuracy of particle size estimation with the measurement uncertainty and the scattering geometry such as the cloud-base height and the lidar sounding depth. Second-order scattering computations are performed for an extended range of particle sizes and for a wide range of lidar fields of view (FOVs). The results obtained allow us to specify the areas of possible applications of these lidars in cloud studies. Comparison of results obtained with polarized and cross-polarized scattered components demonstrate that the cross-polarized signal should provide a more stable retrieval and is preferable when double scattering is highly dominant. Our analysis allows for the estimation of the optimal number of FOVs in the system and their angular distribution, so this work can be a useful tool for practical MFOV lidar design. (c) 2006 Optical Society of America. C1 Inst Gen Phys, Phys Instrumentat Ctr, Moscow 142190, Russia. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Def Res & Dev Canada Valcartier, Val Belair, PQ G3J 1X5, Canada. RP Veselovskii, I (reprint author), Inst Gen Phys, Phys Instrumentat Ctr, Moscow 142190, Russia. EM igorv@quadra.ru; david.whiteman@gsfc.nasa.gov; gilles.roy@drev.dnd.ca RI McGill, Matthew/D-8176-2012 NR 17 TC 11 Z9 12 U1 1 U2 3 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 SEP 10 PY 2006 VL 45 IS 26 BP 6839 EP 6848 DI 10.1364/AO.45.006839 PG 10 WC Optics SC Optics GA 081ZC UT WOS:000240355100027 PM 16926920 ER PT J AU Stecker, FW Malkan, MA Scully, ST AF Stecker, F. W. Malkan, M. A. Scully, S. T. TI Intergalactic photon spectra from the far-IR to the UV Lyman limit for 0 < z < 6 and the optical depth of the universe to high-energy gamma rays SO ASTROPHYSICAL JOURNAL LA English DT Article DE diffuse radiation; gamma rays : observations ID EXTRAGALACTIC BACKGROUND LIGHT; INFRARED LUMINOSITY FUNCTIONS; STAR-FORMING GALAXIES; ULTRA-DEEP-FIELD; SPACE-TELESCOPE; HIGH-REDSHIFT; SPITZER VIEW; PKS 2155-304; COBE FIRAS; MU-M AB We calculate the intergalactic photon density as a function of both energy and redshift for 0 < z < 6 for photon energies from. 003 eV to the Lyman limit cutoff at 13.6 eV in a Lambda CDM universe with Omega(Lambda) = 0.7 and Omega(m) = 0.3. The basic features of our backward-evolution model for galaxies were developed in earlier papers by Malkan & Stecker. With a few improvements, we find that this evolutionary model gives predictions of new deep number counts from Spitzer, as well as a calculation of the spectral energy distribution of the diffuse infrared background, which are in good agreement with the data. We then use our calculated intergalactic photon densities to extend previous work on the absorption of high-energy gamma-rays in intergalactic space owing to interactions with low-energy photons and the 2.7K cosmic microwave background radiation. We calculate the optical depth of the universe, tau, for gamma-rays having energies from 4 GeV to 100 TeV emitted by sources at redshifts from 0 to 5. We also give an analytic fit with numerical coefficients for approximating tau(E gamma; z). As an example of the application of our results, we calculate the absorbed spectrum of the blazar PKS 2155-304 at z = 0.117 and compare it with the spectrum observed by the HESS air Cerenkov gamma-ray telescope array. C1 NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA. James Madison Univ, Dept Phys, Harrisonburg, VA 22807 USA. RP Stecker, FW (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. EM floyd.w.stecker@nasa.gov; malkan@astro.ucla.edu; scullyst@jmu.edu RI Stecker, Floyd/D-3169-2012 NR 84 TC 266 Z9 268 U1 2 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 SEP 10 PY 2006 VL 648 IS 2 BP 774 EP 783 DI 10.1086/506188 PN 1 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 082QZ UT WOS:000240403600002 ER PT J AU Hansen, FK Banday, AJ Eriksen, HK Gorski, KM Lilje, PB AF Hansen, F. K. Banday, A. J. Eriksen, H. K. Gorski, K. M. Lilje, P. B. TI Foreground subtraction of cosmic microwave background maps using WI-FIT (wavelet-based high-resolution fitting of internal templates) SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmic microwave background; cosmology : observations; methods : data analysis; methods : statistical ID PROBE WMAP OBSERVATIONS; ANGULAR POWER SPECTRUM; ASTROPHYSICAL COMPONENT SEPARATION; ANISOTROPY-PROBE; NON-GAUSSIANITY; SPHERICAL WAVELETS; 1ST-YEAR DATA; EMISSION; SKY; RADIATION AB We present a new approach to foreground removal for CMB maps. Rather than relying on prior knowledge about the foreground components, we first extract the necessary information about them directly from the microwave sky maps by taking differences of temperature maps at different frequencies. These difference maps, which we refer to as internal templates, consist only of linear combinations of Galactic foregrounds and noise, with no CMB component. We obtain the foreground-cleaned maps by fitting these internal templates to, and subsequently subtracting the appropriately scaled contributions of them from, the CMB-dominated channels. The fitting operation is performed in wavelet space, making the analysis feasible at high resolution with only a minor loss of precision. Applying this procedure to the WMAP data, we obtain a power spectrum that matches the spectrum obtained by the WMAP team at the signal-dominated scales. The fact that we obtain basically identical results without using any external templates has considerable relevance for future observations of the CMB polarization, where very little is known about the Galactic foregrounds. Finally, we have revisited previous claims about a north-south power asymmetry on large angular scales and confirm that these remain unchanged with this completely different approach to foreground separation. This also holds when fitting the foreground contribution independently to the northern and southern hemisphere, indicating that the asymmetry is unlikely to have its origin in different foreground properties of the hemispheres. This conclusion is further strengthened by the lack of any observed frequency dependence. C1 Univ Oslo, Inst Theoret Astrophys, N-0315 Oslo, Norway. Univ Oslo, Ctr Math Applicat, N-0316 Oslo, Norway. Max Planck Inst Astrophys, D-85741 Garching, Germany. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. Univ Warsaw Observ, PL-00478 Warsaw, Poland. CALTECH, Pasadena, CA 91125 USA. RP Hansen, FK (reprint author), Univ Oslo, Inst Theoret Astrophys, POB 1029, N-0315 Oslo, Norway. EM frodekh@astro.uio.no; banday@mpa-garching.mpg.de; h.k.k.eriksen@astro.uio.no; krzysztof.m.gorski@jpl.nasa.gov; lilje@astro.uio.no RI Lilje, Per/A-2699-2012; OI Lilje, Per/0000-0003-4324-7794 NR 38 TC 31 Z9 31 U1 0 U2 3 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD SEP 10 PY 2006 VL 648 IS 2 BP 784 EP 796 DI 10.1086/506015 PN 1 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 082QZ UT WOS:000240403600003 ER PT J AU Uchiyama, Y Urry, CM Cheung, CC Jester, S Van Duyne, J Coppi, P Sambruna, RM Takahashi, T Tavecchio, F Maraschi, L AF Uchiyama, Yasunobu Urry, C. Megan Cheung, C. C. Jester, Sebastian Van Duyne, Jeffrey Coppi, Paolo Sambruna, Rita M. Takahashi, Tadayuki Tavecchio, Fabrizio Maraschi, Laura TI Shedding new light on the 3C 273 jet with the Spitzer Space Telescope SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : jets; infrared : galaxies; quasars : individual (3C 273); radiation mechanisms : nonthermal ID X-RAY-EMISSION; ACTIVE GALACTIC NUCLEI; LARGE-SCALE JETS; INFRARED ARRAY CAMERA; 3C 273; SYNCHROTRON-RADIATION; RELATIVISTIC JET; EXTRAGALACTIC JETS; SHOCK-WAVES; RADIO JETS AB We have performed infrared imaging of the jet of the quasar 3C 273 at wavelengths of 3.6 and 5.8 mu m with the Infrared Array Camera (IRAC) on the Spitzer Space Telescope. When combined with the radio, optical, and X-ray measurements, the IRAC photometry of the X-ray-bright jet knots clearly shows that the optical emission is dominated by the high-energy emission component of the jet, not by the radio synchrotron component, as had been assumed to date. The high-energy component, represented by a power law from the optical through X-ray, may be due to a second synchrotron component or to inverse Compton scattering of ambient photons. In the former case, we argue that the acceleration of protons exceeding energies of E-p similar to 10(16) eV or possibly even to E-p similar to 10(19) eV would be taking place in the jet knots of 3C 273, assuming that the acceleration time is proportional to the particle gyroradius. In contrast, the inverse Compton model, into which highly relativistic Doppler beaming has to be incorporated, requires very low energy electrons of E-e similar to 1 MeV in the jet knots. The present polarization data in the radio and optical would favor the former interpretation in the case of the 3C 273 jet. Sensitive and detailed measurements of optical polarization are important in order to establish the radiation mechanism responsible for the high-energy emission. The present study offers new clues as to the controversial origin of the X-ray emission seen in many quasar jets. C1 Yale Univ, Yale Ctr Astron & Astrophys, New Haven, CT 06520 USA. Japan Aerosp Explorat Agcy, Inst Space & Astronaut Sci, Sagamihara, Kanagawa 2298510, Japan. Stanford Univ, Kavli Inst Astrophys & Cosmol, Stanford, CA 94305 USA. Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Univ Tokyo, Dept Phys, Tokyo 1130033, Japan. Osserv Astron Brera, I-20121 Milan, Italy. RP Uchiyama, Y (reprint author), Yale Univ, Yale Ctr Astron & Astrophys, 260 Whitney Ave, New Haven, CT 06520 USA. EM uchiyama@astro.isas.jaxa.jp RI Urry, Claudia/G-7381-2011 OI Urry, Claudia/0000-0002-0745-9792 NR 66 TC 46 Z9 46 U1 0 U2 5 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD SEP 10 PY 2006 VL 648 IS 2 BP 910 EP 921 DI 10.1086/505964 PN 1 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 082QZ UT WOS:000240403600014 ER PT J AU Perez-Gonzalez, PG Kennicutt, RC Gordon, KD Misselt, KA de Paz, AG Engelbracht, CW Rieke, GH Bendo, GJ Bianchi, L Boissier, S Calzetti, D Dale, DA Draine, BT Jarrett, TH Hollenbach, D Prescott, MKM AF Perez-Gonzalez, Pablo G. Kennicutt, Robert C., Jr. Gordon, Karl D. Misselt, Karl A. de Paz, Armando Gil Engelbracht, Charles W. Rieke, George H. Bendo, George J. Bianchi, Luciana Boissier, Samuel Calzetti, Daniela Dale, Daniel A. Draine, Bruce T. Jarrett, Thomas H. Hollenbach, David Prescott, Moire K. M. TI Ultraviolet through far-infrared spatially resolved analysis of the recent star formation in M81 (NGC 3031) SO ASTROPHYSICAL JOURNAL LA English DT Review DE dust, extinction; galaxies : ISM; galaxies : individual (M81, NGC 3031); galaxies : photometry; galaxies : spiral; galaxies : stellar content; infrared : galaxies ID H-II REGIONS; SPITZER-SPACE-TELESCOPE; NEARBY GALAXIES SURVEY; SPECTRAL ENERGY-DISTRIBUTIONS; MULTIBAND IMAGING PHOTOMETER; ACTIVE GALACTIC NUCLEI; LARGE-MAGELLANIC-CLOUD; X-RAY-EMISSION; FORMING GALAXIES; STARBURST GALAXIES AB The recent star formation (SF) in the early-type spiral galaxy M81 is characterized using imaging observations from the far-ultraviolet to the far-infrared. We compare these data with models of the stellar, gas, and dust emission for subgalactic regions. Our results suggest the existence of a diffuse dust emission not directly linked to the recent star formation. We find a radial decrease of the dust temperature and dust mass density, and in the attenuation of the stellar light. The IR emission in M81 can be modeled with three components: ( 1) cold dust with a temperature < T(c)> = 18 +/- 2 K, concentrated near the H II regions but also presenting a diffuse distribution; ( 2) warm dust with < T(w)> = 53 +/- 7 K, directly linked with the H II regions; and (3) aromatic molecules, with diffuse morphology peaking around the H II regions. We derive several relationships to obtain total IR luminosities from IR monochromatic fluxes, and we compare five different star formation rate (SFR) estimators for H II regions in M81 and M51: the UV, H alpha, and three estimators based on Spitzer data. We find that the H alpha luminosity absorbed by dust correlates tightly with the 24 mu m emission. The correlation with the total IR luminosity is not as good. Important variations from galaxy to galaxy are found when estimating the total SFR with the 24 mu m or the total IR emission alone. The most reliable estimations of the total SFRs are obtained by combining the H alpha emission (or the UV) and an IR luminosity (especially the 24 mu m emission), which probe the unobscured and obscured SF, respectively. For the entire M81 galaxy, about 50% of the total SF is obscured by dust. The percentage of obscured SF ranges from 60% in the inner regions of the galaxy to 30% in the outer zones. C1 Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. Univ Complutense Madrid, Fac CC Fis, Dept Astrofis, E-28040 Madrid, Spain. Carnegie Inst Washington Observ, Pasadena, CA 91101 USA. Univ London Imperial Coll Sci Technol & Med, Blackett Lab, London SW7 2AZ, England. Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. Traverse Siphon Trios Lucs, Astrophys Lab, F-13376 Marseille 12, France. Space Telescope Sci Inst, Baltimore, MD 21218 USA. Univ Wyoming, Dept Phys & Astron, Laramie, WY 82071 USA. Princeton Univ, Observ, Princeton, NJ 08544 USA. CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA. NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Perez-Gonzalez, PG (reprint author), Univ Arizona, Steward Observ, 933 N Cherry Ave, Tucson, AZ 85721 USA. RI Perez-Gonzalez, Pablo/J-2871-2016; Gil de Paz, Armando/J-2874-2016; OI Perez-Gonzalez, Pablo/0000-0003-4528-5639; Gil de Paz, Armando/0000-0001-6150-2854; Draine, Bruce/0000-0002-0846-936X NR 133 TC 102 Z9 102 U1 0 U2 7 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 SEP 10 PY 2006 VL 648 IS 2 BP 987 EP 1006 PN 1 PG 20 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 082QZ UT WOS:000240403600021 ER PT J AU Krimm, HA Hurkett, C Pal'shin, V Norris, JP Zhang, B Barthelmy, SD Burrows, DN Gehrels, N Golenetskii, S Osborne, JP Parsons, AM Perri, M Willingale, R AF Krimm, H. A. Hurkett, C. Pal'shin, V. Norris, J. P. Zhang, B. Barthelmy, S. D. Burrows, D. N. Gehrels, N. Golenetskii, S. Osborne, J. P. Parsons, A. M. Perri, M. Willingale, R. TI GRB 050717: A long, short-lag, high-peak energy burst observed by Swift and Konus SO ASTROPHYSICAL JOURNAL LA English DT Article DE gamma rays : bursts ID GAMMA-RAY BURSTS; COMPLETE SPECTRAL CATALOG; AFTERGLOW EMISSION; LIGHT CURVES; LUMINOSITY; TELESCOPE; EVOLUTION; MISSION AB The long burst GRB 050717 was observed simultaneously by the Burst Alert Telescope ( BAT) on Swift and the Konus instrument on Wind. Significant hard to soft spectral evolution was seen. Early gamma-ray and X-ray emission was detected by both BAT and the X-Ray Telescope (XRT) on Swift. The XRT continued to observe the burst for 7.1 days and detect it for 1.4 days. The X-ray light curve showed a classic decay pattern; the afterglow was too faint for a jet break to be detected. No optical, infrared, or ultraviolet counterpart was discovered despite deep searches within 14 hr of the burst. Two particular features of the prompt emissionmake GRB 050717 a very unusual burst. First, the peak of the vF(v) spectrum was observed to be 2401(-568)(+781) keV for the main peak, which is the highest value of E-peak ever observed. Second, the spectral lag for GRB 050717 was determined to be 2: 5 +/- 2: 6 ms, consistent with zero and unusually short for a long burst. This lag measurement suggests that this burst has a high intrinsic luminosity and hence is at high redshift ( z > 2.7). Despite these unusual features, GRB 050717 exhibits the classic prompt and afterglow behavior of a gamma-ray burst. C1 NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Univ Space Res Assoc, Columbia, MD 21044 USA. Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England. AF Ioffe Phys Tech Inst, Expt Astrophys Lab, St Petersburg 194021, Russia. Univ Nevada, Dept Phys, Las Vegas, NV 89154 USA. Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. ASI, Sci Data Ctr, I-00044 Frascati, Italy. RP Krimm, HA (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RI Barthelmy, Scott/D-2943-2012; Gehrels, Neil/D-2971-2012; Parsons, Ann/I-6604-2012; Pal'shin, Valentin/F-3973-2014; Golenetskii, Sergey/B-3818-2015; OI Perri, Matteo/0000-0003-3613-4409 NR 53 TC 18 Z9 18 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 SEP 10 PY 2006 VL 648 IS 2 BP 1117 EP 1124 DI 10.1086/506009 PN 1 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 082QZ UT WOS:000240403600033 ER PT J AU Levan, AJ Osborne, JP Tanvir, NR Page, KL Rol, E Zhang, B Goad, MR O'Brien, PT Priddey, RS Bersier, D Burrows, DN Chapman, R Fruchter, AS Giommi, P Gehrels, N Hughes, MA Pak, S Simpson, C Tagliaferri, G Vardoulaki, E AF Levan, A. J. Osborne, J. P. Tanvir, N. R. Page, K. L. Rol, E. Zhang, B. Goad, M. R. O'Brien, P. T. Priddey, R. S. Bersier, D. Burrows, D. N. Chapman, R. Fruchter, A. S. Giommi, P. Gehrels, N. Hughes, M. A. Pak, S. Simpson, C. Tagliaferri, G. Vardoulaki, E. TI The first Swift X-ray flash: The faint afterglow of XRF 050215B SO ASTROPHYSICAL JOURNAL LA English DT Article DE gamma rays : bursts ID BURST ALERT TELESCOPE; ULTRA-VIOLET/OPTICAL TELESCOPE; RELATIVISTIC JETS; ORPHAN AFTERGLOWS; MIDEX MISSION; LIGHT CURVES; SUPERNOVA; REDSHIFT; DISCOVERY; EMISSION AB We present the discovery of XRF 050215B and its afterglow. The burst was detected by the Swift BAT during the check-out phase, and observations with the X-Ray Telescope began approximately 30 minutes after the burst. These observations found a faint, slowly fading X-ray afterglow near the center of the error box as reported by the BAT. Infrared data obtained at UKIRT after 10 hr also revealed a very faint K-band afterglow. The afterglow appears unusual since it is very faint, especially in the infrared, with K > 20 only 9 hr postburst. The X-ray and infrared light curves exhibit a slow, monotonic decay with alpha similar to 0.8 and no evidence for a steepening associated with the jet break to 10 days postburst. We discuss possible explanations for the faintness and slow decay in the context of present models for the production of X-ray flashes. C1 Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England. Univ Hertfordshire, Dept Phys Astron & Math, Hatfield AL9 10AB, Herts, England. Univ Nevada, Dept Phys, Las Vegas, NV 89154 USA. Liverpool John Moores Univ, Astrophys Res Inst, Birkenhead CH41 1LD, Merseyside, England. Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. Space Telescope Sci Inst, Baltimore, MD 21218 USA. ASI, Sci Data Ctr, I-00044 Frascati, Italy. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Liverpool John Moores Univ, Astrophys Res Inst, Birkenhead CH41 1LD, Merseyside, England. INAF, Osservatorio Astron Brera, I-23807 Merate, LC, Italy. Univ Oxford, Dept Phys, Oxford OX1 3RH, England. RP Levan, AJ (reprint author), Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England. RI Gehrels, Neil/D-2971-2012; OI giommi, paolo/0000-0002-2265-5003; Tagliaferri, Gianpiero/0000-0003-0121-0723 NR 82 TC 9 Z9 9 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 SEP 10 PY 2006 VL 648 IS 2 BP 1132 EP 1138 DI 10.1086/506018 PN 1 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 082QZ UT WOS:000240403600035 ER PT J AU Hanasoge, SM Larsen, RM Duvall, TL DeRosa, ML Hurlburt, NE Schou, J Roth, M Christensen-Dalsgaard, J Lele, SK AF Hanasoge, S. M. Larsen, R. M. Duvall, T. L., Jr. DeRosa, M. L. Hurlburt, N. E. Schou, J. Roth, M. Christensen-Dalsgaard, J. Lele, S. K. TI Computational acoustics in spherical geometry: Steps toward validating helioseismology SO ASTROPHYSICAL JOURNAL LA English DT Article DE hydrodynamics; Sun : helioseismology; Sun : interior; Sun : oscillations; waves ID OSCILLATIONS; SCHEMES AB Throughout the past decade, detailed helioseismic analyses of observations of solar surface oscillations have led to advances in our knowledge of the structure and dynamics of the solar interior. Such analyses involve the decomposition of time series of the observed surface oscillation pattern into its constituent wave modes, followed by inversion procedures that yield inferences of properties of the solar interior. While this inverse problem has been a major focus in recent years, the corresponding forward problem has received much less attention. We aim to rectify this situation by taking the first steps toward validating and determining the efficacy of the helioseismic measurement procedure. The goal of this effort is to design a means to perform differential studies of various effects such as flows and thermal perturbations on helioseismic observables such as resonant frequencies, travel-time shifts, etc. Here we describe our first efforts to simulate wave propagation within a spherical shell, which extends from 0.2 to about 1.0004 R-circle dot (where R-circle dot is the radius of the Sun) and which possesses a solar-like stratification. We consider a model containing no flows that will serve as a reference model for later studies. We discuss the computational procedure, some difficulties encountered in a simulation of this kind, and the means to overcome them. We also present techniques used to validate the simulation. C1 Stanford Univ, WW Hansen Expt Lab, Stanford, CA 94305 USA. Stanford Univ, Dept Mech Engn, Stanford, CA 94305 USA. NASA, Goddard Space Flight Ctr, Lab Solar & Space Phys, Greenbelt, MD 20771 USA. Lockheed Martin Solar & Astrophys Lab, Palo Alto, CA 94304 USA. Kiepenheuer Inst Solar Phys, D-79104 Freiburg, Germany. Max Planck Inst Sonnensyst Forsch, D-37191 Katlenburg Lindau, Germany. Aarhus Univ, Inst Fys & Astron, DK-8000 Aarhus, Denmark. RP Hanasoge, SM (reprint author), Stanford Univ, WW Hansen Expt Lab, Stanford, CA 94305 USA. RI Duvall, Thomas/C-9998-2012 NR 15 TC 30 Z9 30 U1 0 U2 3 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD SEP 10 PY 2006 VL 648 IS 2 BP 1268 EP 1275 DI 10.1086/505927 PN 1 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 082QZ UT WOS:000240403600047 ER PT J AU Lane, BF Muterspaugh, MW Shao, M AF Lane, Benjamin F. Muterspaugh, Matthew W. Shao, Michael TI Calibrating an interferometric null SO ASTROPHYSICAL JOURNAL LA English DT Article DE techniques : interferometric ID TERRESTRIAL-PLANET-FINDER AB One of the biggest challenges associated with a nulling-interferometer-based approach to detecting extrasolar Earth-like planets comes from the extremely stringent requirements of path length, polarization, and amplitude matching in the interferometer. To the extent that the light from multiple apertures is not matched in these properties, light will leak through the nuller and confuse the search for a planetary signal. Here we explore the possibility of using the coherence properties of the starlight to separate contributions from the planet and nuller leakage. We find that straightforward modifications to the optical layout of a nulling interferometer will allow one to measure and correct for the leakage to a high degree of precision. This nulling calibration relaxes the field matching requirements substantially and should consequently simplify the instrument design. C1 MIT, Dept Phys, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. CALTECH, Dept Geol & Planetary Sci, Pasadena, CA 91125 USA. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Lane, BF (reprint author), MIT, Dept Phys, Kavli Inst Astrophys & Space Res, 70 Vassar St, Cambridge, MA 02139 USA. EM blane@mit.edu; matthew1@mit.edu; mshao@huey.jpl.nasa.gov NR 12 TC 17 Z9 17 U1 1 U2 5 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD SEP 10 PY 2006 VL 648 IS 2 BP 1276 EP 1284 DI 10.1086/506020 PN 1 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 082QZ UT WOS:000240403600048 ER PT J AU Immler, S Brown, PJ Milne, P The, LS Petre, R Gehrels, N Burrows, DN Nousek, JA Williams, CL Pian, E Mazzali, PA Nomoto, K Chevalier, RA Mangano, V Holland, ST Roming, PWA Greiner, J Pooley, D AF Immler, S. Brown, P. J. Milne, P. The, L. -S. Petre, R. Gehrels, N. Burrows, D. N. Nousek, J. A. Williams, C. L. Pian, E. Mazzali, P. A. Nomoto, K. Chevalier, R. A. Mangano, V. Holland, S. T. Roming, P. W. A. Greiner, J. Pooley, D. TI X-ray observations of Type Ia supernovae with Swift: Evidence of circumstellar interaction for SN 2005ke SO ASTROPHYSICAL JOURNAL LA English DT Article DE circumstellar matter; supernovae : individual (SN 2005ke); ultraviolet : ISM; X-rays : individual (SN 2005ke); X-rays : ISM ID RADIO-EMISSION; LUMINOSITY; SIGNATURES; TELESCOPE; EXPLOSION; PHYSICS AB We present a study of the early ( days to weeks) X-ray and UV properties of eight Type Ia supernovae (SNe Ia) that have been extensively observed with the X-Ray Telescope (XRT) and UV/Optical Telescope (UVOT) on board Swift, ranging from 5 to 132 days after the outburst. SN 2005ke is tentatively detected ( at a 3-3.6 sigma level of significance) in X-rays based on deep monitoring with the XRT ranging from 8 to 120 days after the outburst. The inferred X-ray luminosity [L(0.3-2) (2 +/- 1) x 10(38) ergs s(-1); 0.3-2 keV band] is likely caused by interaction of the SN shock with circumstellar material (CSM) deposited by a stellar wind from the progenitor's companion star with a mass-loss rate of M approximate to 3 x 10(-6) M(circle dot) yr(-1). Evidence of CSM interaction in X- rays is independently confirmed by an excess of UV emission, as observed with the UVOT on board Swift, starting around 35 days after the explosion. The nondetection of SN 2005ke with Chandra 105 days after the outburst implies a rate of decline steeper than, consistent with the decline expected from the interaction L(x) proportional to t(-0.75), of the SN shock with a spherically symmetric CSM (t(-1)). None of the other seven SNe Ia is detected in X-rays or shows a UV excess, which allows us to put tight constraints on the mass-loss rates of the progenitor systems. C1 NASA, Goddard Space Flight Ctr, X Ray Astrophys Lab, Explorat Universe Div, Greenbelt, MD 20771 USA. Univ Space Res Assoc, Columbia, MD 21044 USA. Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. Clemson Univ, Dept Phys & Astron, Clemson, SC 29634 USA. Osserv Astron Trieste, INAF, I-34131 Trieste, Italy. Max Planck Inst Astrophys, D-85741 Garching, Germany. Univ Tokyo, Sch Sci, Dept Astron, Bunkyo Ku, Tokyo 1130033, Japan. Univ Virginia, Dept Astron, Charlottesville, VA 22903 USA. Inst Astrofis Spaziale & Cosm, INAF, I-90146 Palermo, Italy. Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. RP Immler, S (reprint author), NASA, Goddard Space Flight Ctr, X Ray Astrophys Lab, Explorat Universe Div, Code 662, Greenbelt, MD 20771 USA. RI Gehrels, Neil/D-2971-2012; Nomoto, Ken'ichi/A-4393-2011 NR 35 TC 56 Z9 56 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 SEP 10 PY 2006 VL 648 IS 2 BP L119 EP L122 DI 10.1086/507947 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 082RB UT WOS:000240403800009 ER PT J AU Jefferies, SM McIntosh, SW Armstrong, JD Bogdan, TJ Cacciani, A Fleck, B AF Jefferies, Stuart M. McIntosh, Scott W. Armstrong, James D. Bogdan, Thomas J. Cacciani, Alessandro Fleck, Bernhard TI Magnetoacoustic portals and the basal heating of the solar chromosphere SO ASTROPHYSICAL JOURNAL LA English DT Article DE Sun : atmospheric motions; Sun : chromosphere; Sun : magnetic fields ID QUIET-SUN; PHOTOSPHERIC OSCILLATIONS; TRANSITION REGION; ELECTRIC-CURRENTS; MAGNETIC-FIELD; GRAVITY-WAVES; MODELS; ENERGY; CORONA; FREQUENCY AB We show that inclined magnetic field lines at the boundaries of large-scale convective cells (supergranules) provide "portals" through which low-frequency (< 5 mHz) magnetoacoustic waves can propagate into the solar chromosphere. The energy flux carried by these waves at a height of 400 km above the solar surface is found to be a factor of 4 greater than that carried by the high-frequency (> 15 mHz) acoustic waves, which are believed to provide the dominant source of wave heating of the chromosphere. This result opens up the possibility that low-frequency magnetoacoustic waves provide a significant source of energy for balancing the radiative losses of the ambient solar chromosphere. C1 Univ Hawaii, Inst Astron, Kula, HI 96790 USA. SW Res Inst, Dept Space Studies, Boulder, CO 80302 USA. NOAA, Space Environm Ctr, Boulder, CO 80305 USA. Natl Ctr Atmospher Res, High Altitude Observ, Boulder, CO 80307 USA. Univ Roma La Sapienza, Dipartimento Fis, I-00185 Rome, Italy. NASA, Goddard Space Flight Ctr, ESA, Res & Sci Support Dept, Greenbelt, MD 20771 USA. RP Jefferies, SM (reprint author), Univ Hawaii, Inst Astron, 4761 Lower Kula Rd, Kula, HI 96790 USA. RI Fleck, Bernhard/C-9520-2012 NR 34 TC 107 Z9 108 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD SEP 10 PY 2006 VL 648 IS 2 BP L151 EP L155 DI 10.1086/508165 PN 2 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 082RB UT WOS:000240403800017 ER PT J AU Postigo, AD Castro-Tirado, AJ Guziy, S Gorosabel, J Johannesson, G Aloy, MA McBreen, S Lamb, DQ Benitez, N Jelinek, M Pandey, SB Coe, D Perez-Ramirez, MD Aceituno, FJ Alises, M Acosta-Pulido, JA Gomez, G Lopez, R Donaghy, TQ Nakagawa, YE Sakamoto, T Ricker, GR Hearty, FR Bayliss, M Gyuk, G York, DG AF Postigo, A. de Ugarte Castro-Tirado, A. J. Guziy, S. Gorosabel, J. Johannesson, G. Aloy, M. A. McBreen, S. Lamb, D. Q. Benitez, N. Jelinek, M. Pandey, S. B. Coe, D. Perez-Ramirez, M. D. Aceituno, F. J. Alises, M. Acosta-Pulido, J. A. Gomez, G. Lopez, R. Donaghy, T. Q. Nakagawa, Y. E. Sakamoto, T. Ricker, G. R. Hearty, F. R. Bayliss, M. Gyuk, G. York, D. G. TI GRB 060121: Implications of a short-/intermediate-duration gamma-ray burst at high redshift SO ASTROPHYSICAL JOURNAL LA English DT Article DE gamma rays : bursts ID DIGITAL SKY SURVEY; AFTERGLOW; GALAXY; GRB-050709; ENERGY; DUST; GRB; EMISSION; MERGERS; COLORS AB Since the discovery of the first short-population g-ray burst (GRB) afterglows in 2005, the handful of observed events have been found to be embedded in nearby (z < 1), bright underlying galaxies. We present multiwavelength observations of GRB 060121, the first short burst observed to clearly outshine its host galaxy ( by a factor 1102). A photometric redshift for this event places the progenitor at a most probable redshift of z p 4.6, with a less probable scenario of z = 1.7. In either case, GRB 060121 could be the farthermost short-population GRB detected to date and implies an isotropic-equivalent energy release in gamma rays comparable to that seen in long-population bursts. We discuss the implications of the released energy on the nature of the progenitor. These results suggest that GRB 060121 may belong to a family of energetic short-population events, lying at z 1 1 and whose optical afterglows would outshine their host galaxies, unlike the first short GRBs observed in 2005. The possibility of GRB 060121 being an intermediate-duration burst is also discussed. C1 CSIC, IAA, E-18008 Granada, Spain. Nikolaev State Univ, UA-54030 Nikolayev, Ukraine. Univ Iceland, Inst Sci, IS-107 Reykjavik, Iceland. Max Planck Inst Astrophys, D-85741 Garching, Germany. Univ Valencia, Dept Astron & Astrofis, E-46100 Burjassot, Spain. Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA. Univ Jaen, Dept Fis, EPS, E-23071 Jaen, Spain. Calar Alto Observ, E-04080 Almeria, Spain. Inst Astrofis Canarias, E-38200 San Cristobal la Laguna, Tenerife, Spain. Univ Barcelona, Dept Astron & Meteorol, E-08028 Barcelona, Spain. Aoyama Gakuin Univ, Dept Phys & Math, Sagamihara, Kanagawa 2298558, Japan. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. MIT, Kavli Inst, Cambridge, MA 02139 USA. Univ Colorado, Ctr Astrophys & Space Astron, Boulder, CO 80303 USA. RP Postigo, AD (reprint author), CSIC, IAA, Camino Bajo de Huetor 50, E-18008 Granada, Spain. RI Aloy, Miguel/K-9941-2014; Johannesson, Gudlaugur/O-8741-2015; Jelinek, Martin/E-5290-2016; OI Aloy, Miguel/0000-0002-5552-7681; Johannesson, Gudlaugur/0000-0003-1458-7036; Jelinek, Martin/0000-0003-3922-7416; de Ugarte Postigo, Antonio/0000-0001-7717-5085 NR 50 TC 39 Z9 39 U1 1 U2 5 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD SEP 10 PY 2006 VL 648 IS 2 BP L83 EP L87 DI 10.1086/507868 PN 2 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 082RB UT WOS:000240403800001 ER PT J AU Terada, Y Mihara, T Nakajima, M Suzuki, M Isobe, N Makishima, K Takahashi, H Enoto, T Kokubun, M Kitaguchi, T Naik, S Dotani, T Nagase, F Tanaka, T Watanabe, S Kitamoto, S Sudoh, K Yoshida, A Nakagawa, Y Sugita, S Kohmura, T Kotani, T Yonetoku, D Angelini, L Cottam, J Mukai, K Kelley, R Soong, Y Bautz, M Kissel, S Doty, J AF Terada, Y. Mihara, T. Nakajima, M. Suzuki, M. Isobe, N. Makishima, K. Takahashi, H. Enoto, T. Kokubun, M. Kitaguchi, T. Naik, S. Dotani, T. Nagase, F. Tanaka, T. Watanabe, S. Kitamoto, S. Sudoh, K. Yoshida, A. Nakagawa, Y. Sugita, S. Kohmura, T. Kotani, T. Yonetoku, D. Angelini, L. Cottam, J. Mukai, K. Kelley, R. Soong, Y. Bautz, M. Kissel, S. Doty, J. TI Cyclotron resonance energies at a low X-ray luminosity: A0535+262 observed with Suzaku SO ASTROPHYSICAL JOURNAL LA English DT Article DE magnetic fields; pulsars : individual ( A0535+26); stars : neutron; X-rays : binaries ID PULSAR 4U-0115+63; TIMING-EXPLORER; LINE; ASTRO-E2; OUTBURST AB The binary X-ray pulsar A0535 + 262 was observed with the Suzaku X-ray observatory on 2005 September 14 for a net exposure of 22 ks. The source was in the declining phase of a minor outburst, exhibiting 3-50 keV luminosity of similar to 3.7 x 10(35) ergs s(-1) at an assumed distance of 2 kpc. In spite of the very low source intensity ( about 30 mcrab at 20 keV), its electron cyclotron resonance was detected clearly with the Suzaku Hard X-Ray Detector, in absorption at about 45 keV. The resonance energy is found to be essentially the same as that measured when the source is almost 2 orders of magnitude more luminous. These results are compared with the luminosity-dependent changes in the cyclotron resonance energy, observed from 4U 0115 + 63 and X0331 + 53. C1 Inst Phys & Chem Res, Cosm Radiat Lab, Wako, Saitama 3510198, Japan. Univ Tokyo, Dept Phys, Bunkyo Ku, Tokyo 1130033, Japan. JAXA, Inst Space & Astronaut Sci, Sagamihara, Kanagawa 2298510, Japan. Rikkyo Univ, Dept Phys, Toshima Ku, Tokyo 1718501, Japan. Aoyama Gakuin Univ, Dept Math & Phys, Sagamihara, Kanagawa 2298558, Japan. Kogakuin Univ, Dept Phys, Hachioji, Tokyo 1920015, Japan. Tokyo Tech, Dept Phys, Meguro Ku, Tokyo 1528551, Japan. Kanazawa Univ, Dept Phys, Kanazawa, Ishikawa 9201192, Japan. NASA, Goddard Space Flight Ctr, Explorat Universe Div, Greenbelt, MD 20771 USA. MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. Noqsi Aerosp Ltd, Pine, CO 80470 USA. RP Terada, Y (reprint author), Inst Phys & Chem Res, Cosm Radiat Lab, Wako, Saitama 3510198, Japan. RI Terada, Yukikatsu/A-5879-2013; XRAY, SUZAKU/A-1808-2009; Mihara, Tatehiro/C-5536-2017 OI Terada, Yukikatsu/0000-0002-2359-1857; Mihara, Tatehiro/0000-0002-6337-7943 NR 23 TC 34 Z9 34 U1 0 U2 4 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD SEP 10 PY 2006 VL 648 IS 2 BP L139 EP L142 DI 10.1086/508018 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 082RB UT WOS:000240403800014 ER PT J AU Maktav, D Gutman, G AF Maktav, Dr Derya Gutman, Dr Garik TI Preface SO INTERNATIONAL JOURNAL OF REMOTE SENSING LA English DT Editorial Material C1 NASA, Washington, DC 20546 USA. RP Maktav, D (reprint author), NASA, Washington, DC 20546 USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU TAYLOR & FRANCIS LTD PI ABINGDON PA 4 PARK SQUARE, MILTON PARK, ABINGDON OX14 4RN, OXON, ENGLAND SN 0143-1161 J9 INT J REMOTE SENS JI Int. J. Remote Sens. PD SEP 10 PY 2006 VL 27 IS 17 BP 3625 EP 3626 DI 10.1080/01431160500500284 PG 2 WC Remote Sensing; Imaging Science & Photographic Technology SC Remote Sensing; Imaging Science & Photographic Technology GA 090LU UT WOS:000240953600001 ER PT J AU Chopping, MJ Su, LH Laliberte, A Rango, A Peters, DPC Martonchik, JV AF Chopping, Mark J. Su, Lihong Laliberte, Andrea Rango, Albert Peters, Debra P. C. Martonchik, John V. TI Mapping woody plant cover in desert grasslands using canopy reflectance modeling and MISR data SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID BIDIRECTIONAL REFLECTANCE; ENCROACHMENT AB A simplified geometric-optical model (SGM) was inverted using red band reflectance data acquired at 275 m in nine viewing angles from the Multiangle Imaging SpectroRadiometer (MISR) flown on NASA's Terra satellite, to provide estimates of fractional woody plant cover for large areas (over 3519 km 2) in parts of the Chihuahuan Desert in New Mexico, USA. The use of the model in these semi-arid environments was enabled by the derivation of a priori estimates of the soil/understory background reflectance response. This was made possible by determining relationships between the kernel weights from a LiSparse-RossThin model adjusted against the same MISR data - together with spectral reflectance data derived from MISR's nadir-viewing camera - and the parameters of the Walthall model used to represent the background. Spatial distributions of retrieved fractional woody plant cover match those of % tree cover in the global MODIS Vegetation Continuous Fields product but also include shrubs. Good relationships were obtained with fractional shrub cover measured in pastures in the USDA, ARS Jornada Experimental Range but tree cover in higher elevation and riparian zones was dramatically overestimated as a result of the fixing of crown height and shape parameters. C1 Montclair State Univ, Dept Earth & Environm Studies, Montclair, NJ 07043 USA. Agr Res Serv, USDA, Jornada Expt Range, Las Cruces, NM 88003 USA. NASA, Jet Prop Lab, Pasadena, CA 91109 USA. RP Chopping, MJ (reprint author), Montclair State Univ, Dept Earth & Environm Studies, Montclair, NJ 07043 USA. EM choppingm@pegasus.montclair.edu NR 13 TC 12 Z9 14 U1 0 U2 3 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD SEP 9 PY 2006 VL 33 IS 17 AR L17402 DI 10.1029/2006GL027148 PG 5 WC Geosciences, Multidisciplinary SC Geology GA 082WN UT WOS:000240418000010 ER PT J AU Douglass, AR Stolarski, RS Strahan, SE Polansky, BC AF Douglass, A. R. Stolarski, R. S. Strahan, S. E. Polansky, B. C. TI Sensitivity of Arctic ozone loss to polar stratospheric cloud volume and chlorine and bromine loading in a chemistry and transport model SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID GENERAL-CIRCULATION MODEL; 3-DIMENSIONAL MODEL; AURA SATELLITE; EOS MLS; ART.; VORTEX AB The sensitivity of Arctic ozone loss to polar stratospheric cloud volume (V(PSC)) and chlorine and bromine loading is explored using chemistry and transport models (CTMs). One simulation uses multi-decadal winds and temperatures from a general circulation model (GCM). Winter polar ozone loss depends on both equivalent effective stratospheric chlorine (EESC) and polar vortex characteristics (temperatures, descent, isolation, polar stratospheric cloud amount). The simulation reproduces a linear relationship between ozone loss and V(PSC) in agreement with that derived from observations for 1992-2003. The relationship holds for EESC within similar to 85% of its maximum (similar to 1990-2020). For lower EESC the ozone loss varies linearly with EESC unless V(PSC) similar to 0. A second simulation recycles a single year's winds and temperatures from the GCM so that polar ozone loss depends only on changes in EESC. This simulation shows that ozone loss varies linearly with EESC for the entire EESC range for constant, high V(PSC). C1 NASA, Atmospher Chem & Dynam Branch, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Univ Maryland Baltimore Cty, Goddard Earth Sci & Technol Ctr, Baltimore, MD 21228 USA. Sci Syst & Applicat Inc, Lanham, MD 20706 USA. RP Douglass, AR (reprint author), NASA, Atmospher Chem & Dynam Branch, Goddard Space Flight Ctr, Code 613-3, Greenbelt, MD 20771 USA. EM anne.r.douglass@nasa.gov RI Douglass, Anne/D-4655-2012; Strahan, Susan/H-1965-2012; Stolarski, Richard/B-8499-2013 OI Stolarski, Richard/0000-0001-8722-4012 NR 22 TC 10 Z9 11 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 SEP 9 PY 2006 VL 33 IS 17 AR L17809 DI 10.1029/2006GL026492 PG 5 WC Geosciences, Multidisciplinary SC Geology GA 082WN UT WOS:000240418000003 ER PT J AU Matsui, T Masunaga, H Kreidenweis, SM Pielke, RA Tao, WK Chin, M Kaufman, YJ AF Matsui, Toshihisa Masunaga, Hirohiko Kreidenweis, Sonia M. Pielke, Roger A., Sr. Tao, Wei-Kuo Chin, Mian Kaufman, Yoram J. TI Satellite-based assessment of marine low cloud variability associated with aerosol, atmospheric stability, and the diurnal cycle SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID MARITIME LOW CLOUDS; LIQUID WATER PATH; BOUNDARY-LAYER; VISIBLE/INFRARED SCANNER; PHYSICAL-PROPERTIES; MICROWAVE IMAGER; TROPICAL OCEANS; CLIMATE SYSTEM; OPTICAL DEPTH; GOCART MODEL AB This study examines variability in marine low cloud properties derived from semiglobal observations by the Tropical Rainfall Measuring Mission (TRMM) satellite, as linked to the aerosol index (AI) and lower-tropospheric stability (LTS). AI is derived from the Moderate Resolution Imaging Spectroradiometer (Terra MODIS) sensor and the Goddard Chemistry Aerosol Radiation and Transportation (GOCART) model and is used to represent column-integrated aerosol concentrations. LTS is derived from the NCEP/NCAR reanalysis and represents the background thermodynamic environment in which the clouds form. Global statistics reveal that cloud droplet size tends to be smallest in polluted (high-AI) and strong inversion (high-LTS) environments. Statistical quantification shows that cloud droplet size is better correlated with AI than it is with LTS. Simultaneously, the cloud liquid water path (CLWP) tends to decrease as AI increases. This correlation does not support the hypothesis or assumption that constant or increased CLWP is associated with high aerosol concentrations. Global variability in corrected cloud albedo (CCA), the product of cloud optical depth and cloud fraction, is very well explained by LTS, while both AI and LTS are needed to explain local variability in CCA. Most of the local correlations between AI and cloud properties are similar to the results from the global statistics, while weak anomalous aerosol-cloud correlations appear locally in the regions where simultaneous high (low) AI and low (high) LTS compensate each other. Daytime diurnal cycles explain additional variability in cloud properties. CCA has the largest diurnal cycle in high-LTS regions. Cloud droplet size and CLWP have weak diurnal cycles that differ between clean and polluted environments. The combined results suggest that investigations of marine low cloud radiative forcing and its relationship to hypothesized aerosol indirect effects must consider the combined effects of aerosols, thermodynamics, and the diurnal cycle. C1 Colorado State Univ, Dept Atmospher Sci, Ft Collins, CO 80523 USA. NASA, Goddard Space Flight Ctr, Atmospheres Lab, Greenbelt, MD 20771 USA. RP Matsui, T (reprint author), Colorado State Univ, Dept Atmospher Sci, Ft Collins, CO 80523 USA. EM matsuit@atmos.colostate.edu RI Masunaga, Hirohiko/C-2488-2008; Pielke, Roger/A-5015-2009; Chin, Mian/J-8354-2012; PMM, JAXA/K-8537-2016; Kreidenweis, Sonia/E-5993-2011 OI Masunaga, Hirohiko/0000-0002-6336-5002; Kreidenweis, Sonia/0000-0002-2561-2914 NR 50 TC 54 Z9 54 U1 0 U2 15 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X EI 2169-8996 J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD SEP 9 PY 2006 VL 111 IS D17 AR D17204 DI 10.1029/2005JD006097 PG 16 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 082XN UT WOS:000240420600001 ER PT J AU Yang, ES Cunnold, DM Salawitch, RJ McCormick, MP Russell, J Zawodny, JM Oltmans, S Newchurch, MJ AF Yang, Eun-Su Cunnold, Derek M. Salawitch, Ross J. McCormick, M. Patrick Russell, James, III Zawodny, Joseph M. Oltmans, Samuel Newchurch, Michael J. TI Attribution of recovery in lower-stratospheric ozone SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID HALOGEN OCCULTATION EXPERIMENT; BALLOON-BORNE MEASUREMENTS; EXPERIMENT II MEASUREMENTS; TREND ANALYSIS; UARS PLATFORM; DOBSON SPECTROPHOTOMETERS; GEOPHYSICAL CONDITIONS; EUROPEAN VALIDATION; INSTRUMENTS ABOARD; EARTHS ATMOSPHERE AB Multiple satellite and ground-based observations provide consistent evidence that the thickness of Earth's protective ozone layer has stopped declining since 1997, close to the time of peak stratospheric halogen loading. Regression analyses with Effective Equivalent Stratospheric Chlorine (EESC) in conjunction with further analyses using more sophisticated photochemical model calculations constrained by satellite data demonstrate that the cessation of ozone depletion between 18 and 25 km altitude is consistent with a leveling off of stratospheric abundances of chlorine and bromine, due to the Montreal Protocol and its amendments. However, ozone increases in the lowest part of the stratosphere, from the tropopause to 18 km, account for about half of the improvement in total column ozone during the past 9 years at Northern Hemisphere midlatitudes. The increase in ozone for altitudes below 18 km is most likely driven by changes in transport, rather than driven by declining chlorine and bromine. Even with this evidence that the Montreal Protocol and its amendments are having the desired, positive effect on ozone above 18 km, total column ozone is recovering faster than expected because of the apparent transport driven changes at lower altitudes. Accurate prediction of future levels of stratospheric ozone will require comprehensive understanding of the factors that drive temporal changes at various altitudes and partitioning of the recent transport-driven increases between natural variability and changes in atmospheric structure perhaps related to anthropogenic climate change. C1 Georgia Inst Technol, Sch Earth & Atmospher Sci, Atlanta, GA 30332 USA. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. Hampton Univ, Ctr Atmospher Sci, Hampton, VA 23668 USA. NASA, Langley Res Ctr, Hampton, VA 23681 USA. NOAA, Earth Syst Res Lab, Global Monitoring Div, Boulder, CO 80305 USA. Univ Alabama, Dept Atmospher Sci, Huntsville, AL 35805 USA. RP Yang, ES (reprint author), Georgia Inst Technol, Sch Earth & Atmospher Sci, 311 Ferst Dr, Atlanta, GA 30332 USA. EM mike@nsstc.uah.edu RI Salawitch, Ross/B-4605-2009 OI Salawitch, Ross/0000-0001-8597-5832 NR 95 TC 48 Z9 49 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 SEP 9 PY 2006 VL 111 IS D17 AR D17309 DI 10.1029/2005JD006371 PG 21 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 082XN UT WOS:000240420600003 ER PT J AU Marsh, DR Smith, AK Mlynczak, MG Russell, JM AF Marsh, Daniel R. Smith, Anne K. Mlynczak, Martin G. Russell, James M., III TI SABER observations of the OH Meinel airglow variability near the mesopause SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article ID LOWER THERMOSPHERE; ROTATIONAL TEMPERATURES; SEASONAL VARIABILITY; ATMOSPHERIC TIDES; HYDROXYL AIRGLOW; OZONE MAXIMUM; GRAVITY-WAVES; LOW LATITUDES; MESOSPHERE; MODEL AB [ 1] The Sounding of the Atmosphere using Broadband Emission Radiometry (SABER) instrument, one of four on board the TIMED satellite, observes the OH Meinel emission at 2.0 mu m that peaks near the mesopause. The emission results from reactions between members of the oxygen and hydrogen chemical families that can be significantly affected by mesopause dynamics. In this study we compare SABER measurements of OH Meinel emission rates and temperatures with predictions from a three-dimensional chemical dynamical model. In general, the model is capable of reproducing both the observed diurnal and seasonal OH Meinel emission variability. The results indicate that the diurnal tide has a large effect on the overall magnitude and temporal variation of the emission in low latitudes. This tidal variability is so dominant that the seasonal cycle in the nighttime emission depends very strongly on the local time of the analysis. At higher latitudes the emission has an annual cycle that is due mainly to transport of oxygen by the seasonally reversing mean circulation. C1 Natl Ctr Atmospher Res, Div Atmospher Chem, Boulder, CO 80307 USA. Hampton Univ, Ctr Atmospher Sci, Hampton, VA 23668 USA. NASA, Langley Res Ctr, Hampton, VA 23681 USA. RP Marsh, DR (reprint author), Natl Ctr Atmospher Res, Div Atmospher Chem, POB 3000, Boulder, CO 80307 USA. EM marsh@ucar.edu; aksmith@ucar.edu RI Marsh, Daniel/A-8406-2008; Mlynczak, Martin/K-3396-2012 OI Marsh, Daniel/0000-0001-6699-494X; NR 34 TC 45 Z9 46 U1 1 U2 5 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9380 EI 2169-9402 J9 J GEOPHYS RES-SPACE JI J. Geophys. Res-Space Phys. PD SEP 9 PY 2006 VL 111 IS A10 AR A10S05 DI 10.1029/2005JA011451 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 083AL UT WOS:000240428200001 ER PT J AU Stolarski, RS Frith, SM AF Stolarski, R. S. Frith, S. M. TI Search for evidence of trend slow-down in the long-term TOMS/SBUV total ozone data record: the importance of instrument drift uncertainty SO ATMOSPHERIC CHEMISTRY AND PHYSICS LA English DT Article ID SOLAR BACKSCATTER ULTRAVIOLET; STRATOSPHERIC OZONE; TRANSPORT MODEL; CALIBRATION; INCREASES; CHLORINE; TOMS AB We have developed a merged ozone data set ( MOD) for the period October 1978 through June 2006 combining total ozone measurements ( Version 8 retrieval) from the TOMS ( Nimbus 7, Earth Probe) and SBUV/SBUV2 ( Nimbus 7, NOAA 9/11/16) series of satellite instruments. We use the MOD data set to search for evidence of ozone recovery in response to the observed leveling off of chlorine and bromine compounds in the stratosphere. A crucial step in any time series analysis is the evaluation of uncertainties. In addition to the standard statistical time series uncertainties, we evaluate the possible instrument drift uncertainty for the MOD data set. We combine these two sources of uncertainty and apply them to a cumulative sum of residuals (CUSUM) analysis for trend slow-down. For the extra-polar mean between 60 degrees S and 60 degrees N, the apparent slow-down in trend is found to be clearly significant if instrument uncertainties are ignored. When instrument uncertainties are added, the slow-down becomes marginally significant at the 2 sigma level. For the mid-latitudes of the northern hemisphere (30 degrees to 60 degrees N) the trend slow-down is highly significant at the 2 sigma level, while in the southern hemisphere the trend slow-down has yet to meet the 2 sigma significance criterion. The rate of change of chlorine/bromine compounds is similar in both hemispheres, and we expect the ozone response to be similar in both hemispheres as well. The asymmetry in the trend slow-down between hemispheres likely reflects the influence of dynamical variability, and thus a clearly statistically significant response of total ozone to the leveling off of chlorine and bromine in the stratosphere is not yet indicated. C1 NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Sci Syst & Applicat Inc, Lanham, MD 20706 USA. RP Stolarski, RS (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. EM stolar@polska.gsfc.nasa.gov RI Stolarski, Richard/B-8499-2013 OI Stolarski, Richard/0000-0001-8722-4012 NR 29 TC 83 Z9 85 U1 0 U2 1 PU COPERNICUS PUBLICATIONS PI KATHLENBURG-LINDAU PA MAX-PLANCK-STR 13, KATHLENBURG-LINDAU, 37191, GERMANY SN 1680-7316 J9 ATMOS CHEM PHYS JI Atmos. Chem. Phys. PD SEP 8 PY 2006 VL 6 BP 4057 EP 4065 PG 9 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 083WU UT WOS:000240489700001 ER PT J AU Chang, YF Jalbout, AF Zhang, JP Su, ZM Wang, RS AF Chang, Yingfei Jalbout, Abraham F. Zhang, Jingping Su, Zhongmin Wang, Rongshun TI Theoretical study on C-32 fullerenes and derivatives SO CHEMICAL PHYSICS LETTERS LA English DT Article ID SMALLEST FULLERENE; CARBON CLUSTERS; C-60; STABILITY; CAGES; C-70; C-24; NANOTUBES; OLIGOMERS; CHEMISTRY AB A series of B3LYP/6-31G* calculations reveal that the D-3 isomer is the most stable isomer of C-32 carbon cages. The derivatives of it, including additional productions (C32H2, C32Cl2), hetero-fullerenes (C30B2, C30N2), isoelectronic molecules (C30B22-, C30N22+) and dimers have been investigated at the same level. The results show that, the additional hydrogen atoms and replaced nitrogen atoms can enhance the electronic stabilization of D3C32. Our calculations suggest that the building block of C-32 oligomers which linked by sp(3) bonds should be the saturated C32H2 unit. (c) 2006 Elsevier B.V. All rights reserved. C1 NE Normal Univ, Fac Chem, Inst Funct Mat Chem, Changchun 130024, Peoples R China. Univ Arizona, NASA, Astrobiol Ctr, Tucson, AZ 85721 USA. Univ Arizona, Dept Chem, Tucson, AZ 85721 USA. RP Wang, RS (reprint author), NE Normal Univ, Fac Chem, Inst Funct Mat Chem, Changchun 130024, Peoples R China. EM wangrs@nenu.edu.cn RI Su, Zhong-Min/H-4734-2011; Zhang, Jingping/C-1312-2014 OI Zhang, Jingping/0000-0001-8004-3673 NR 35 TC 11 Z9 15 U1 0 U2 4 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0009-2614 J9 CHEM PHYS LETT JI Chem. Phys. Lett. PD SEP 8 PY 2006 VL 428 IS 1-3 BP 148 EP 151 DI 10.1016/j.cplett.2006.06.091 PG 4 WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical SC Chemistry; Physics GA 082NB UT WOS:000240392400029 ER PT J AU Drake, NB Tamppari, LK Baker, RD Cantor, BA Hale, AS AF Drake, Nathan B. Tamppari, Leslie K. Baker, R. David Cantor, Bruce A. Hale, Amy S. TI Dust devil tracks and wind streaks in the North Polar Region of Mars: A study of the 2007 Phoenix Mars Lander Sites SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID ORBITER CAMERA; VARIABLE FEATURES; ART. AB The 65 - 72 latitude band of the North Polar Region of Mars, where the 2007 Phoenix Mars Lander will land, was studied using satellite images from the Mars Global Surveyor (MGS) Mars Orbiter Camera Narrow-Angle (MOC-NA) camera. Dust devil tracks (DDT) and wind streaks (WS) were observed and recorded as surface evidence for winds. No active dust devils (DDs) were observed. 162 MOC-NA images, 10.3% of total images, contained DDT/WS. Phoenix landing Region C ( 295 - 315W) had the highest concentration of images containing DDT/WS per number of available images (20.9%); Region D ( 130 - 150W) had the lowest (3.5%). DDT and WS direction were recorded for Phoenix landing regions A ( 110 - 130W), B ( 240 - 260W), and C to infer local wind direction. Region A showed dominant northwest-southeast DDT/WS, Region B showed dominant north-south, east-west and northeast-southwest DDT/WS, and region C showed dominant west/northwest-east/southeast DDT/ WS. Results indicate the 2007 Phoenix Lander has the highest probability of landing near DDT/ WS in landing Region C. Based on DDT/ WS linearity, we infer Phoenix would likely encounter directionally consistent background wind in any of the three regions. C1 Austin Coll, Dept Phys, Sherman, TX 75090 USA. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. Malin Space Sci Syst, San Diego, CA 92191 USA. RP Drake, NB (reprint author), Austin Coll, Dept Phys, Sherman, TX 75090 USA. EM nathan.drake@gmail.com NR 19 TC 12 Z9 12 U1 0 U2 2 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 EI 1944-8007 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD SEP 8 PY 2006 VL 33 IS 19 AR L19S02 DI 10.1029/2006GL026270 PG 4 WC Geosciences, Multidisciplinary SC Geology GA 082WQ UT WOS:000240418300001 ER PT J AU Millet, DB Jacob, DJ Turquety, S Hudman, RC Wu, SL Fried, A Walega, J Heikes, BG Blake, DR Singh, HB Anderson, BE Clarke, AD AF Millet, Dylan B. Jacob, Daniel J. Turquety, Solene Hudman, Rynda C. Wu, Shiliang Fried, Alan Walega, James Heikes, Brian G. Blake, Donald R. Singh, Hanwant B. Anderson, Bruce E. Clarke, Antony D. TI Formaldehyde distribution over North America: Implications for satellite retrievals of formaldehyde columns and isoprene emission SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID OZONE MONITORING EXPERIMENT; SECONDARY ORGANIC AEROSOLS; NITROGEN-OXIDE EMISSIONS; TROPOSPHERIC NO2 COLUMNS; DIODE-LASER MEASUREMENTS; GOME MEASUREMENTS; UNITED-STATES; ATMOSPHERIC CHEMISTRY; BIOGENIC EMISSIONS; OXIDATION-PRODUCTS AB [1] Formaldehyde ( HCHO) columns measured from space provide constraints on emissions of volatile organic compounds (VOCs). Quantitative interpretation requires characterization of errors in HCHO column retrievals and relating these columns to VOC emissions. Retrieval error is mainly in the air mass factor (AMF) which relates fitted backscattered radiances to vertical columns and requires external information on HCHO, aerosols, and clouds. Here we use aircraft data collected over North America and the Atlantic to determine the local relationships between HCHO columns and VOC emissions, calculate AMFs for HCHO retrievals, assess the errors in deriving AMFs with a chemical transport model (GEOS-Chem), and draw conclusions regarding space-based mapping of VOC emissions. We show that isoprene drives observed HCHO column variability over North America; HCHO column data from space can thus be used effectively as a proxy for isoprene emission. From observed HCHO and isoprene profiles we find an HCHO molar yield from isoprene oxidation of 1.6 +/- 0.5, consistent with current chemical mechanisms. Clouds are the primary error source in the AMF calculation; errors in the HCHO vertical profile and aerosols have comparatively little effect. The mean bias and 1 sigma uncertainty in the GEOS- Chem AMF calculation increase from < 1% and 15% for clear skies to 17% and 24% for half-cloudy scenes. With fitting errors, this gives an overall 1 sigma error in HCHO satellite measurements of 25 - 31%. Retrieval errors, combined with uncertainties in the HCHO yield from isoprene oxidation, result in a 40% (1 sigma) error in inferring isoprene emissions from HCHO satellite measurements. C1 Harvard Univ, Dept Earth & Planetary Sci, Cambridge, MA 02138 USA. Harvard Univ, Div Engn & Appl Sci, Cambridge, MA 02138 USA. Natl Ctr Atmospher Res, Earth Observing Lab, Boulder, CO 80307 USA. Univ Rhode Isl, Grad Sch Oceanog, Narragansett, RI 02882 USA. Univ Calif Irvine, Dept Chem, Irvine, CA 92697 USA. NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. NASA, Langley Res Ctr, Div Atmospher Sci, Hampton, VA 23681 USA. Univ Hawaii Manoa, Sch Ocean & Earth Sci & Technol, Honolulu, HI 96822 USA. RP Millet, DB (reprint author), Harvard Univ, Dept Earth & Planetary Sci, 20 Oxford St, Cambridge, MA 02138 USA. EM dbm@io.harvard.edu RI Hudman, Rynda/C-6118-2009; Millet, Dylan/G-5832-2012; White, Allen/A-7946-2009; Goldstein, Allen/A-6857-2011; Chem, GEOS/C-5595-2014 OI Goldstein, Allen/0000-0003-4014-4896; NR 92 TC 92 Z9 92 U1 3 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 SEP 8 PY 2006 VL 111 IS D24 AR D24S02 DI 10.1029/2005JD006853 PG 17 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 082XP UT WOS:000240420800001 ER PT J AU Treffeisen, RE Thomason, LW Strom, J Herber, AB Burton, SP Yamanouchi, T AF Treffeisen, R. E. Thomason, L. W. Stroem, J. Herber, A. B. Burton, S. P. Yamanouchi, T. TI Stratospheric Aerosol and Gas Experiment (SAGE) II and III aerosol extinction measurements in the Arctic middle and upper troposphere SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID EXPERIMENT-II MEASUREMENTS; SAGE-II; SIZE DISTRIBUTION; OPTICAL-PROPERTIES; ART.; CLIMATOLOGY; RADIATION; SVALBARD; PATTERNS; CLOUD AB In recent years, substantial effort has been expended toward understanding the impact of tropospheric aerosols on Arctic climate and chemistry. A significant part of this effort has been the collection and documentation of extensive aerosol physical and optical property data sets. However, the data sets present significant interpretive challenges because of the diverse nature of these measurements. Among the longest continuous records is that by the spaceborne Stratospheric Aerosol and Gas Experiment (SAGE) II. Although SAGE tropospheric measurements are restricted to the middle and upper troposphere, they may be able to provide significant insight into the nature and variability of tropospheric aerosol, particularly when combined with ground and airborne observations. This paper demonstrates the capacity of aerosol products from SAGE II and its follow-on experiment SAGE III to describe the temporal and vertical variations of Arctic aerosol characteristics. We find that the measurements from both instruments are consistent enough to be combined. Using this combined data set, we detect a clear annual cycle in the aerosol extinction for the middle and upper Arctic troposphere. C1 Alfred Wegener Inst Polar & Marine Res, D-14473 Potsdam, Germany. NASA, Langley Res Ctr, Hampton, VA 23681 USA. Stockholm Univ, Dept Appl Environm Sci, SE-10691 Stockholm, Sweden. Alfred Wegener Inst Polar & Marine Res, D-27570 Bremerhaven, Germany. Natl Inst Polar Res, Tokyo 1738515, Japan. RP Treffeisen, RE (reprint author), Alfred Wegener Inst Polar & Marine Res, Telegrafenberg A45, D-14473 Potsdam, Germany. EM rtreff@awi-potsdam.de; l.w.thomason@nasa.gov; johan@itm.su.se; aherber@awi-bremerhaven.de; yamanou@pmg.nipr.ac.jp RI Yamanouchi, Takashi/P-2041-2015 NR 48 TC 7 Z9 8 U1 0 U2 5 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X EI 2169-8996 J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD SEP 8 PY 2006 VL 111 IS D17 AR D17203 DI 10.1029/2005JD006271 PG 12 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 082XK UT WOS:000240420300001 ER PT J AU Squyres, SW Knoll, AH Arvidson, RE Clark, BC Grotzinger, JP Jolliff, BL McLennan, SM Tosca, N Bell, JF Calvin, WM Farrand, WH Glotch, TD Golombek, MP Herkenhoff, KE Johnson, JR Klingelhofer, G McSween, HY Yen, AS AF Squyres, S. W. Knoll, A. H. Arvidson, R. E. Clark, B. C. Grotzinger, J. P. Jolliff, B. L. McLennan, S. M. Tosca, N. Bell, J. F., III Calvin, W. M. Farrand, W. H. Glotch, T. D. Golombek, M. P. Herkenhoff, K. E. Johnson, J. R. Klingelhoefer, G. McSween, H. Y. Yen, A. S. TI Two years at Meridiani Planum: Results from the Opportunity Rover SO SCIENCE LA English DT Article ID BURNS FORMATION; MARS; FLOWS; ENVIRONMENT; DIAGENESIS; DEPOSITS; ORIGIN AB The Mars Exploration Rover Opportunity has spent more than 2 years exploring Meridiani Planum, traveling similar to 8 kilometers and detecting features that reveal ancient environmental conditions. These include well-developed festoon ( trough) cross-lamination formed in flowing liquid water, strata with smaller and more abundant hematite-rich concretions than those seen previously, possible relict "hopper crystals'' that might reflect the formation of halite, thick weathering rinds on rock surfaces, resistant fracture fills, and networks of polygonal fractures likely caused by dehydration of sulfate salts. Chemical variations with depth show that the siliciclastic fraction of outcrop rock has undergone substantial chemical alteration from a precursor basaltic composition. Observations from microscopic to orbital scales indicate that ancient Meridiani once had abundant acidic groundwater, arid and oxidizing surface conditions, and occasional liquid flow on the surface. C1 Cornell Univ, Dept Astron, Ithaca, NY 14853 USA. Harvard Univ, Bot Museum, Cambridge, MA 02138 USA. Washington Univ, Dept Earth & Planetary Sci, St Louis, MO 63031 USA. Lockheed Martin Corp, Littleton, CO 80127 USA. CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. SUNY Stony Brook, Dept Geosci, Stony Brook, NY 11794 USA. Univ Nevada, Reno, NV 89557 USA. Space Sci Inst, Boulder, CO 80301 USA. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. US Geol Survey, Flagstaff, AZ 86001 USA. Johannes Gutenberg Univ Mainz, Inst Anorgan & Analyt Chem, D-55099 Mainz, Germany. Univ Tennessee, Dept Earth & Planetary Sci, Knoxville, TN 37996 USA. RP Squyres, SW (reprint author), Cornell Univ, Dept Astron, Space Sci Bldg, Ithaca, NY 14853 USA. RI Glotch, Timothy/B-6829-2008; Johnson, Jeffrey/F-3972-2015 NR 34 TC 116 Z9 116 U1 1 U2 21 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 SEP 8 PY 2006 VL 313 IS 5792 BP 1403 EP 1407 DI 10.1126/science.1130890 PG 5 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 081WQ UT WOS:000240348700033 PM 16959999 ER PT J AU Raymond, SN Mandell, AM Sigurdsson, S AF Raymond, Sean N. Mandell, Avi M. Sigurdsson, Steinn TI Exotic Earths: Forming habitable worlds with giant planet migration SO SCIENCE LA English DT Article ID SUN-LIKE STARS; TERRESTRIAL PLANETS; ORBITAL MIGRATION; MASS; ACCRETION; SYSTEMS; GROWTH; PROTOPLANETS; EVOLUTION AB Close-in giant planets (e.g., "hot Jupiters'') are thought to form far from their host stars and migrate inward, through the terrestrial planet zone, via torques with a massive gaseous disk. Here we simulate terrestrial planet growth during and after giant planet migration. Several-Earth-mass planets also form interior to the migrating jovian planet, analogous to recently discovered "hot Earths.'' Very-water-rich, Earth-mass planets form from surviving material outside the giant planet's orbit, often in the habitable zone and with low orbital eccentricities. More than a third of the known systems of giant planets may harbor Earth-like planets. C1 Univ Colorado, Atmospher & Space Phys Lab, Boulder, CO 80309 USA. Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Raymond, SN (reprint author), Univ Colorado, Atmospher & Space Phys Lab, Campus Box 392, Boulder, CO 80309 USA. EM raymond@lasp.colorado.edu; mandell@astro.psu.edu RI Mandell, Avi/F-9361-2012; OI Sigurdsson, Steinn/0000-0002-8187-1144 NR 35 TC 113 Z9 115 U1 1 U2 6 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 SEP 8 PY 2006 VL 313 IS 5792 BP 1413 EP 1416 DI 10.1126/science.1130461 PG 4 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 081WQ UT WOS:000240348700035 PM 16960000 ER PT J AU Forbes, KF St Cyr, OC AF Forbes, Kevin F. St. Cyr, O. C. TI Reply to comment by John G. Kappenman on ''Space weather and the electricity market: An initial assessment'' SO SPACE WEATHER-THE INTERNATIONAL JOURNAL OF RESEARCH AND APPLICATIONS LA English DT Editorial Material ID CURRENTS C1 Catholic Univ Amer, Dept Econ & Business, Washington, DC 20064 USA. Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Forbes, KF (reprint author), Catholic Univ Amer, Dept Econ & Business, 620 Michigan Ave NE, Washington, DC 20064 USA. EM forbes@cua.edu OI Forbes, Kevin/0000-0002-9521-6845 NR 11 TC 2 Z9 2 U1 0 U2 3 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 1542-7390 J9 SPACE WEATHER JI Space Weather PD SEP 8 PY 2006 VL 4 IS 9 AR S09003 DI 10.1029/2005SW000172 PG 4 WC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology & Atmospheric Sciences SC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology & Atmospheric Sciences GA 083FZ UT WOS:000240443100002 ER PT J AU Nghiem, SV Chao, Y Neumann, G Li, P Perovich, DK Street, T Clemente-Colon, P AF Nghiem, S. V. Chao, Y. Neumann, G. Li, P. Perovich, D. K. Street, T. Clemente-Colon, P. TI Depletion of perennial sea ice in the East Arctic Ocean SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID POLARIMETRIC SIGNATURES; PHYSICAL-PROPERTIES; FRAM STRAIT; ALGORITHM; EXTENT; SHELF; COVER AB The extent of perennial sea ice in the East Arctic Ocean ( 0 - 180 degrees E) decreased by nearly one half with an abrupt reduction of 0.95 x 10(6) km(2), while the West Arctic Ocean (0 - 180 degrees W) had a slight gain of 0.23 x 10(6) km(2) between 2004 and 2005, as observed by satellite scatterometer data during November - December. The net decrease in the total perennial ice extent is 0.72 x 10(6) km(2), about the size of Texas. Perennial ice in the East Arctic Ocean continued to be depleted with an areal reduction of 70% from October 2005 to April 2006. With the East Arctic Ocean dominated by seasonal sea ice, a strong summer melt may open a vast ice-free region with a possible record minimum ice extent largely confined to the West Arctic Ocean. Simultaneous scatterometer measurements of sea ice and winds will be crucial for sea ice monitoring and forecasts. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. Natl Ice Ctr, Washington, DC 20385 USA. USA, Cold Reg Res & Engn Lab, Hanover, NH 03755 USA. RP Nghiem, SV (reprint author), CALTECH, Jet Prop Lab, MS 300-325,4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM son.v.nghiem@jpl.nasa.gov RI Clemente-Colon, Pablo/F-5581-2010 NR 36 TC 52 Z9 52 U1 1 U2 5 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 SEP 7 PY 2006 VL 33 IS 17 AR L17501 DI 10.1029/2006GL027198 PG 6 WC Geosciences, Multidisciplinary SC Geology GA 082WE UT WOS:000240417100008 ER PT J AU Glotch, TD Bandfield, JL Christensen, PR Calvin, WM McLennan, SM Clark, BC Rogers, AD Squyres, SW AF Glotch, Timothy D. Bandfield, Joshua L. Christensen, Philip R. Calvin, Wendy M. McLennan, Scott M. Clark, Benton C. Rogers, A. Deanne Squyres, Steven W. TI Mineralogy of the light-toned outcrop at Meridiani Planum as seen by the Miniature Thermal Emission Spectrometer and implications for its formation SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Article ID PLAYA EVAPORITE MINERALS; OPPORTUNITY ROVER; RIO-TINTO; HEMATITE MINERALIZATION; ACIDIC ENVIRONMENT; SPECTRAL EVIDENCE; SOUTHWEST SPAIN; BURNS FORMATION; MARTIAN SOIL; LANDING SITE AB [ 1] Analysis of Miniature Thermal Emission Spectrometer (Mini-TES) data has led to the recovery of a pure end-member spectral shape related to the light-toned outcrop observed at Meridiani Planum. Data from the MER Mossbauer spectrometer, APXS, and previous Mini-TES measurements were used to constrain a spectral library used to determine the mineralogy of the outcrop from this spectral shape. Linear deconvolution of the outcrop spectral shape suggests that it is composed primarily of Al-rich opaline silica, Mg-, Ca-, and Fe-bearing sulfates, plagioclase feldspar, nontronite, and hematite. Conversion of modeled mineralogy to chemistry shows good agreement with the chemical composition of the outcrops determined by APXS. Details of the analysis procedure and implications for the formation of the outcrop are discussed along with terrestrial analogs of the ancient environment at Meridiani. C1 CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. Arizona State Univ, Dept Geol Sci, Tempe, AZ USA. Univ Nevada, Dept Geol Sci, Reno, NV USA. SUNY Stony Brook, Dept Geosci, Stony Brook, NY 11794 USA. Lockheed Martin Space Syst, Denver, CO USA. Cornell Univ, Dept Astron, Ithaca, NY 14853 USA. RP Glotch, TD (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM tglotch@gps.caltech.edu RI Glotch, Timothy/B-6829-2008 NR 94 TC 77 Z9 78 U1 1 U2 9 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 SEP 7 PY 2006 VL 111 IS E12 AR E12S03 DI 10.1029/2005JE002672 PG 14 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 082YY UT WOS:000240424300001 ER PT J AU Squyres, SW Aharonson, O Arvidson, RE Bell, JF Christensen, PR Clark, BC Crisp, JA Farrand, W Glotch, T Golombek, MP Grant, J Grotzinger, J Herkenhoff, KE Johnson, JR Jolliff, BL Knoll, AH McLennan, SM McSween, HY Moore, JM Rice, JW Tosca, N AF Squyres, S. W. Aharonson, O. Arvidson, R. E. Bell, J. F., III Christensen, P. R. Clark, B. C. Crisp, J. A. Farrand, W. Glotch, T. Golombek, M. P. Grant, J. Grotzinger, J. Herkenhoff, K. E. Johnson, J. R. Jolliff, B. L. Knoll, A. H. McLennan, S. M. McSween, H. Y. Moore, J. M. Rice, J. W., Jr. Tosca, N. TI Bedrock formation at Meridiani Planum SO NATURE LA English DT Letter ID BURNS FORMATION; MARS; ENVIRONMENT; DIAGENESIS C1 Cornell Univ, Dept Astron, Ithaca, NY 14853 USA. CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. Washington Univ, Dept Earth & Planetary Sci, St Louis, MO 63130 USA. Arizona State Univ, Dept Geol Sci, Tempe, AZ 85287 USA. Lockheed Martin Corp, Littleton, CO 80127 USA. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. Space Sci Inst, Boulder, CO 80301 USA. Smithsonian Inst, Ctr Earth & Planetary Studies, Washington, DC 20560 USA. US Geol Survey, Flagstaff, AZ 86001 USA. Harvard Univ, Bot Museum, Cambridge, MA 02138 USA. SUNY Stony Brook, Dept Geosci, Stony Brook, NY 11794 USA. Univ Tennessee, Dept Earth & Planetary Sci, Knoxville, TN 37996 USA. NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Squyres, SW (reprint author), Cornell Univ, Dept Astron, Ithaca, NY 14853 USA. EM squyres@astro.cornell.edu RI Johnson, Jeffrey/F-3972-2015; Crisp, Joy/H-8287-2016 OI Crisp, Joy/0000-0002-3202-4416 NR 11 TC 15 Z9 15 U1 0 U2 2 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 0028-0836 J9 NATURE JI Nature PD SEP 7 PY 2006 VL 443 IS 7107 BP E1 EP E2 DI 10.1038/nature05212 PG 2 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 081JM UT WOS:000240313900033 PM 16957684 ER PT J AU Lowe, D MacKenzie, AR Schlager, H Voigt, C Dornbrack, A Mahoney, MJ Cairo, F AF Lowe, D. MacKenzie, A. R. Schlager, H. Voigt, C. Doernbrack, A. Mahoney, M. J. Cairo, F. TI Liquid particle composition and heterogeneous reactions in a mountain wave Polar Stratospheric Cloud SO ATMOSPHERIC CHEMISTRY AND PHYSICS LA English DT Article ID NITRIC-ACID TRIHYDRATE; LARGE HNO3-CONTAINING PARTICLES; ARCTIC STRATOSPHERE; SULFURIC-ACID; LIDAR OBSERVATIONS; VAPOR-PRESSURES; GRAVITY-WAVES; OZONE LOSS; AEROSOL; MODEL AB Mountain wave polar stratospheric clouds (PSCs) were detected on 8 February 2003 above the Scandinavian Mountains by in-situ instruments onboard the M55 Geophysica aircraft. PSC particle composition, backscatter and chlorine activation for this case are studied with a recently developed non-equilibrium microphysical box model for liquid aerosol. Results from the microphysical model, run on quasi-lagrangian trajectories, show that the PSC observed was composed of supercooled ternary (H2O/HNO3/H2SO4) solution (STS) particles, which are out of equilibrium with the gas phase. The measured condensed nitric acid and aerosol backscatter of the PSC can well be simulated with the model. Up to 0.15 ppbv Cl-2 can be released by the PSC within 2 h, showing the propensity of these small-scale clouds for chlorine activation. Equilibrium calculations - of the sort commonly used in large scale chemistry transport models - overestimate the measured condensed nitrate by up to a factor of 3, and overestimates chlorine activation by 10%, in this mountain wave cloud. C1 Univ Lancaster, Dept Environm Sci, Lancaster, England. DLR, Inst Atmospher Phys, Oberpfaffenhofen, Germany. CALTECH, Jet Prop Lab, Pasadena, CA USA. CNR, ISAC, Rome, Italy. RP MacKenzie, AR (reprint author), Univ Lancaster, Dept Environm Sci, Lancaster, England. EM r.mackenzie@lancaster.ac.uk RI Voigt, Christiane/G-3279-2010; MacKenzie, Angus Robert/B-1704-2009; cairo, francesco/C-7460-2015 OI MacKenzie, Angus Robert/0000-0002-8227-742X; cairo, francesco/0000-0002-2886-2601 NR 54 TC 10 Z9 10 U1 1 U2 5 PU COPERNICUS GESELLSCHAFT MBH PI GOTTINGEN PA BAHNHOFSALLEE 1E, GOTTINGEN, 37081, GERMANY SN 1680-7316 EI 1680-7324 J9 ATMOS CHEM PHYS JI Atmos. Chem. Phys. PD SEP 6 PY 2006 VL 6 BP 3611 EP 3623 PG 13 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 083WT UT WOS:000240489600001 ER PT J AU Tran, N Vandemark, D Chapron, B Labroue, S Feng, H Beckley, B Vincent, P AF Tran, N. Vandemark, D. Chapron, B. Labroue, S. Feng, H. Beckley, B. Vincent, P. TI New models for satellite altimeter sea state bias correction developed using global wave model data SO JOURNAL OF GEOPHYSICAL RESEARCH-OCEANS LA English DT Article ID WIND-SPEED ALGORITHM; ELECTROMAGNETIC BIAS; RADAR ALTIMETRY; IN-SITU; OCEAN; LEVEL; TOPEX; CURRENTS; CLIMATE; SLOPE AB [ 1] Changing surface wave conditions alter the altimeter's estimate of mean sea level. Present-day methods for correcting this bias are solely based on wave and wind information from the altimeter. This paper tests the use of additional information to develop several sea state bias correction models using a yearlong combination of Jason-1 data with wave field statistics generated from the WaveWatch3 ocean wave model hindcast. Each candidate model is produced in the same manner, using a nonparametric mapping between Jason-1 sea surface height anomaly estimates and two correlatives. The first is always the significant wave height from Jason-1 and the model differences come through choice of the second variable. Past studies dictate our selection of these second parameters and they include terms related to the local wind speed, swell energy, wave age, wave period, and wave slope. Model skills are evaluated in terms of explained variance. Several models indicate promise for wave model use in future empirical developments. For instance, results show that in the low latitudes the models developed using the swell height and mean period modestly but systematically outperform the actual operational parameterisation. This study further indicates that systematic regional error in the present sea level corrections may be improved by inclusion of wave model information. C1 CLS, Space Oceanog Div, F-31520 Ramonville St Agne, France. NASA, Goddard Space Flight Ctr, Wallops Isl, VA 23337 USA. IFREMER, Ctr Brest, F-29280 Plouzane, France. Hampton Univ, Ctr Atmospher Sci, Hampton, VA 23668 USA. Raytheon Informat Technol & Sci Serv, Landover, MD 20774 USA. CNES, Toulouse, France. RP Tran, N (reprint author), CLS, Space Oceanog Div, 8-10 Rue Hermes, F-31520 Ramonville St Agne, France. EM tran@cls.fr RI Chapron, Bertrand/O-6527-2015 NR 40 TC 8 Z9 10 U1 0 U2 2 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0148-0227 J9 J GEOPHYS RES-OCEANS JI J. Geophys. Res.-Oceans PD SEP 6 PY 2006 VL 111 IS C9 AR C09009 DI 10.1029/2005JC003406 PG 16 WC Oceanography SC Oceanography GA 082YA UT WOS:000240421900002 ER PT J AU Wu, XP Heflin, MB Ivins, ER Fukumori, I AF Wu, Xiaoping Heflin, Michael B. Ivins, Erik R. Fukumori, Ichiro TI Seasonal and interannual global surface mass variations from multisatellite geodetic data SO JOURNAL OF GEOPHYSICAL RESEARCH-SOLID EARTH LA English DT Article ID TIME-VARIABLE GRAVITY; SEA-LEVEL; GEOCENTER VARIATIONS; GPS DATA; EARTH; FIELD; DEFORMATION; VARIABILITY; SYSTEM; MOTION AB [ 1] Monthly global surface mass distribution changes are estimated in the spherical harmonic domain with a complete spectrum up to degree and order 50. The estimates are derived by inverting GPS displacement series measured at roughly 450 continuously tracking sites and ocean bottom pressure (OBP) estimates of a data assimilated ocean circulation model from 1993 to 2004. The inversion uses a hybrid estimator after singular value decomposition of the normalized measurement equations with reduced reliance on a priori spectral information. The results are then compared and combined with Gravity Recovery and Climate Experiment ( GRACE) gravity data to provide enhanced spectral and geographic coverage. High fidelity degree-1 surface mass variation coefficients are recovered, corresponding to equivalent geocenter motion with better than 0.5 mm annual amplitude precisions in all three components. A clear annual surface mass cycle occurs in both GPS/OBP- and GRACE-derived results. There is very good agreement among the low-degree spherical harmonic coefficients and in global geographic pattern but with significant regional differences in amplitudes. Annual variations of average mass over the global oceans, Antarctica, and Greenland are then derived. Total surface mass over both Antarctica and Greenland peak in their respective summers due to increased atmospheric mass. Large interannual variations have also been found involving several continents in the 11-year GPS/OBP solution. The patterns of variation suggest that the recent satellite laser ranging (SLR) observation of a reversal in trend of the Earth's oblateness may be largely an interannual surface mass cycle with considerable contribution from the northern continents. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Wu, XP (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr,MS 238-600, Pasadena, CA 91109 USA. EM xiaoping.wu@jpl.nasa.gov; mbh@mail.jpl.nasa.gov; eri@fryxell.jpl.nasa.gov; if@pacific.jpl.nasa.gov NR 52 TC 52 Z9 52 U1 2 U2 17 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9313 EI 2169-9356 J9 J GEOPHYS RES-SOL EA JI J. Geophys. Res.-Solid Earth PD SEP 6 PY 2006 VL 111 IS B9 AR B09401 DI 10.1029/2005JB004100 PG 20 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 082ZK UT WOS:000240425500003 ER PT J AU Fuerstenau, SD AF Fuerstenau, Stephen D. TI Solar heating of suspended particles and the dynamics of Martian dust devils SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID MARS PATHFINDER; SIMULATIONS; ATMOSPHERE; VORTICES AB The heat input to Martian dust devils due to solar warming of suspended particles is assessed based on a prior estimate of dust loading and from an analysis of shadows cast by dust devils in images taken from orbit. Estimated values for solar heating range from 0.12 to 0.57 W/m(3) with associated temperature increases of 0.011 to 0.051 degrees C per second. These warming rates are comparable to the adiabatic cooling rate expected for a gas parcel rising on Mars with a vertical velocity of 10 m/s. Solar warming of suspended dust serves to maintain buoyancy in a rising dust plume and may be one cause for the large scale of dust devils observed on Mars. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Fuerstenau, SD (reprint author), CALTECH, Jet Prop Lab, MS 306-336,4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM stephen.fuerstenau@jpl.nasa.gov NR 18 TC 21 Z9 21 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 SEP 2 PY 2006 VL 33 IS 19 AR L19S03 DI 10.1029/2006GL026798 PG 4 WC Geosciences, Multidisciplinary SC Geology GA 081QL UT WOS:000240332000001 ER PT J AU de Goncalves, LGG Shuttleworth, WJ Chou, SC Xue, YK Houser, PR Toll, DL Marengo, J Rodell, M AF Goncalves de Goncalves, L. Gustavo Shuttleworth, William James Chou, Sin Chan Xue, Yongkang Houser, Paul R. Toll, David L. Marengo, Jose Rodell, Matthew TI Impact of different initial soil moisture fields on Eta model weather forecasts for South America SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID LAND DATA ASSIMILATION; CONVECTIVE ADJUSTMENT SCHEME; BOUNDARY LAYER INTERACTIONS; SIMPLE BIOSPHERE MODEL; REGIONAL-MODEL; TROPOSPHERIC CIRCULATION; BRIGHTNESS TEMPERATURE; ATMOSPHERIC CONTROLS; SURFACE MODEL; PRECIPITATION AB [ 1] Two 7-day weather simulations were made for South America in July 2003 and January 2004 ( in the Southern Hemisphere summer and winter) to investigate the impacts of using different soil moisture initialization fields in the Eta model coupled to the Simplified Simple Biosphere (SSiB) land surface model. The alternative initial soil moisture fields were ( 1) the soil moisture climatology used operationally by the Centro de Previsao do Tempo e Estudos Climaticos in Brazil and ( 2) the soil moisture fields generated by a South American Land Data Assimilation System (SALDAS) based on SSiB. When the SALDAS soil moisture fields were used, there was an increase in the model performance relative to climatology in the equitable threat score calculated with respect to observed surface precipitation fields and a decrease ( up to 53%) in the root-mean-square error relative to the NCEP analysis of the modeled geopotential height at 500 hPa and mean sea level pressure. However, there was small change in the model skill in positioning the primary South American weather systems because of a change in the upper troposphere circulation caused by SALDAS initialization, most noticeably in the South Atlantic Convergence Zone. C1 Univ Arizona, Dept Hydrol & Water Resources, Tucson, AZ 85721 USA. Inst Nacl Pesquisas Espaciais, Ctr Previsao Tempo & Estudios Climat, BR-12630000 Sao Paulo, Brazil. Univ Calif Los Angeles, Dept Geog, Los Angeles, CA 90095 USA. George Mason Univ, Ctr Res Environm & Water, Beltsville, MD 20705 USA. NASA, Goddard Space Flight Ctr, Hydrol Sci Branch, Greenbelt, MD 20771 USA. RP de Goncalves, LGG (reprint author), NASA, Goddard Space Flight Ctr, Hydrol Sci Branch, Code 614-3, Greenbelt, MD 20771 USA. EM gustavo@hsb.gsfc.nasa.gov RI Rodell, Matthew/E-4946-2012; Marengo, Jose /J-9382-2012; de Goncalves, Luis Gustavo/G-2522-2012; Houser, Paul/J-9515-2013; Chou, Sin Chan/F-6364-2012; OI Rodell, Matthew/0000-0003-0106-7437; Marengo, Jose /0000-0002-8154-2762; Houser, Paul/0000-0002-2991-0441; Chou, Sin Chan/0000-0002-8973-1808; de Goncalves, Luis Gustavo/0000-0002-1571-0916 NR 63 TC 16 Z9 16 U1 0 U2 4 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X EI 2169-8996 J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD SEP 2 PY 2006 VL 111 IS D17 AR D17102 DI 10.1029/2005JD006309 PG 14 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 081RD UT WOS:000240333800001 ER PT J AU Matson, DL Davies, AG Veeder, GJ Rathbun, JA Johnson, TV Castillo, JC AF Matson, Dennis L. Gerard Davies, Ashley Veeder, Glenn J. Rathbun, Julie A. Johnson, Torrence V. Castillo, Julie C. TI Io: Loki Patera as a magma sea SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Article ID THERMAL EMISSION; KILAUEA VOLCANO; SILICATE VOLCANISM; TIDAL DISSIPATION; ACTIVE VOLCANISM; GALILEO NIMS; SULFUR FLOWS; LAVA FLOWS; HEAT-FLOW; HOT-SPOTS AB [1] We develop a physical model for Loki Patera as a magma sea. We calculate the total volume of magma moving through the Loki Patera volcanic system every resurfacing cycle (similar to 540 days) and the resulting variation in thermal emission. The rate of magma solidification at times reaches 3 x 10(6) kg s(-1), with a total solidified volume averaging 100 km(3) yr(-1). A simulation of gas physical chemistry evolution yields the crust porosity profile and the timescale when it will become dense enough to founder in a manner consistent with observations. The Loki Patera surface temperature distribution shows that different areas are at different life cycle stages. On a regional scale, however, there can be coordinated activity, indicated by the wave of thermal change which progresses from Loki Patera's SW quadrant toward the NE at a rate of similar to 1 km d(-1). Using the observed surface temperature distribution, we test several mechanisms for resurfacing Loki Patera, finding that resurfacing with lava flows is not realistic. Only the crustal foundering process is consistent with observations. These tests also discovered that sinking crust has a "heat deficit'' which promotes the solidification of additional magma onto the sinking plate ("bulking up''). In the limiting case, the mass of sinking material can increase to a mass of similar to 3 times that of the foundering plate. With all this solid matter sinking, there is a compensating upward motion in the liquid magma. This can be in excess of 2 m yr(-1). In this manner, solid-liquid convection is occurring in the sea. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. Univ Redlands, Dept Phys, Redlands, CA 92373 USA. RP Matson, DL (reprint author), CALTECH, Jet Prop Lab, MS 183-501,4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM ashley.g.davies@jpl.nasa.gov NR 51 TC 21 Z9 21 U1 2 U2 6 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 SEP 2 PY 2006 VL 111 IS E9 AR E09002 DI 10.1029/2006JE002703 PG 21 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 081SD UT WOS:000240336400003 ER PT J AU Semmel, GS Davis, SR Leucht, KW Rowe, DA Smith, KE O'Farrell, R Boloni, L AF Semmel, Glenn S. Davis, Steven R. Leucht, Kurt W. Rowe, Dan A. Smith, Kevin E. O'Farrell, Ryan Boeloeni, Ladislau TI NESTA: NASA Engineering Shuttle Telemetry Agent SO AI MAGAZINE LA English DT Article; Proceedings Paper CT 1st International Conference on Human-Robot Interaction CY MAR 02-04, 2006 CL Salt Lake City, UT AB The Electrical Systems Division at the NASA Kennedy Space Center has developed and deployed an agent-based tool to monitor the space shuttle's ground processing telemetry stream. The application, the NASA Engineering Shuttle Telemetry Agent (NESTA), increases situational awareness for system and hardware engineers during ground processing of the shuttle's subsystems. The agent provides autonomous monitoring of the telemetry stream and automatically alerts system engineers when predefined criteria have been met. Efficiency and safety are improved through increased automation. Sandia National Labs' Java Expert System Shell is employed as the rule engine. The shell's predicate logic lends itself well to capturing the heuristics and specifying the engineering rules of this spaceport domain. The declarative paradigm of the rule-based agent yields a highly modular and scalable design spanning multiple subsystems of the shuttle. Several hundred monitoring rules have been written thus far with corresponding notifications sent to shuttle engineers. This article discusses the rule-based telemetry agent used for space shuttle ground processing and explains the problem domain, development of the agent software, benefits of AI technology, and deployment and sustaining engineering of the product. C1 NASA, Engn Dev Directorate, KSC, Kennedy Space Ctr, FL 32899 USA. NASA, Engn Shuttle Telemetry Agent Project, Kennedy Space Ctr, FL USA. NASA, Shuttle Proc Directorate, KSC, Kennedy Space Ctr, FL 32899 USA. Auburn Univ, Auburn, AL 36849 USA. Univ Cent Florida, Dept Comp Engn, Orlando, FL 32816 USA. RP Semmel, GS (reprint author), NASA, Engn Dev Directorate, KSC, Mail Code DX-E1, Kennedy Space Ctr, FL 32899 USA. EM Glenn.S.Semmel@nasa.gov; Steve.Davis@nasa.gov; Kurt.Leucht@nasa.gov; Daniel.A.Rowe@nasa.gov; Kevin.E.Smith@nasa.gov; John.R.Ofarrell@nasa.gov NR 12 TC 0 Z9 0 U1 0 U2 0 PU AMER ASSOC ARTIFICIAL INTELL PI MENLO PK PA 445 BURGESS DRIVE, MENLO PK, CA 94025-3496 USA SN 0738-4602 J9 AI MAG JI AI Mag. PD FAL PY 2006 VL 27 IS 3 BP 25 EP 35 PG 11 WC Computer Science, Artificial Intelligence SC Computer Science GA 090EP UT WOS:000240933700003 ER PT J AU Rybski, PE Tejada, S Blank, D Stroupe, A Bugajska, M Greenwald, L AF Rybski, Paul E. Tejada, Sheila Blank, Douglas Stroupe, Ashley Bugajska, Magdalena Greenwald, Lloyd TI The AAAI 2005 Mobile Robot Competition and Exhibition SO AI MAGAZINE LA English DT Article; Proceedings Paper CT 1st International Conference on Human-Robot Interaction CY MAR 02-04, 2006 CL Salt Lake City, UT AB The Fourteenth Annual AAAI Mobile Robot Competition and Exhibition was held at the National Conference on Artificial Intelligence in Pittsburgh, Pennsylvania, in July 2005. This year marked a change in the venue format from a conference hall to a hotel, which changed how the robot event was run. As a result, the robots were much more visible to the attendees of the AAAI conference than in previous years. This allowed teams that focused on human-robot interaction to have many more opportunities to interact with people. This article describes the events that were held at the conference, including the Scavenger Hunt, Open Interaction, Robot Challenge, and Robot Exhibition. C1 Carnegie Mellon Univ, Inst Robot, Pittsburgh, PA 15213 USA. Bryn Mawr Coll, Bryn Mawr, PA 19010 USA. CALTECH, Jet Prop Lab, Mars Explorat Rover Project, Pasadena, CA USA. USN, Ctr Appl Res Artificial Intelligence, Washington, DC USA. Drexel Univ, Intelligent Time Crit Syst Lab, Philadelphia, PA USA. RP Rybski, PE (reprint author), Carnegie Mellon Univ, Inst Robot, Pittsburgh, PA 15213 USA. EM prybski@cs.cmu.edu; dblank@cs.brynmawr.edu; magda@aic.nrl.navy.mil NR 5 TC 1 Z9 1 U1 0 U2 0 PU AMER ASSOC ARTIFICIAL INTELL PI MENLO PK PA 445 BURGESS DRIVE, MENLO PK, CA 94025-3496 USA SN 0738-4602 J9 AI MAG JI AI Mag. PD FAL PY 2006 VL 27 IS 3 BP 85 EP 102 PG 18 WC Computer Science, Artificial Intelligence SC Computer Science GA 090EP UT WOS:000240933700008 ER PT J AU Panda, J Seasholtz, RG AF Panda, J. Seasholtz, R. G. TI Experimental investigation of Reynolds and Favre averaging in high-speed jets 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 LAYERS; NOISE AB Recent advancements in a molecular Rayleigh scattering based diagnostic technique allowed for simultaneous measurement of velocity and density fluctuations with high sampling rates. The technique was used to investigate unheated high subsonic and supersonic fully expanded free jets in the Mach number range from 0.8 to 1.8. The difference between the Favre-averaged and the Reynolds-averaged axial velocity and axial component of the turbulent kinetic energy is found to be small. On average, estimates based on Morkovin's strong Reynolds analogy are found to underpredict turbulent density fluctuations. C1 Ohio Aerosp Inst, Brookpark, OH 44135 USA. NASA, John H Glenn Res Ctr Lewis Field, Acoust Branch, Brookpark, OH 44135 USA. RP Panda, J (reprint author), NASA, John H Glenn Res Ctr Lewis Field, Acoust Branch, Brookpark, OH 44135 USA. NR 14 TC 2 Z9 2 U1 0 U2 4 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 SEP PY 2006 VL 44 IS 9 BP 1952 EP 1959 DI 10.2514/1.15638 PG 8 WC Engineering, Aerospace SC Engineering GA 082UQ UT WOS:000240413100004 ER PT J AU Bryson, S Levy, D AF Bryson, Steve Levy, Doron TI Mapped WENO and weighted power ENO reconstructions in semi-discrete central schemes for Hamilton-Jacobi equations SO APPLIED NUMERICAL MATHEMATICS LA English DT Article; Proceedings Paper CT Workshop on Numerical Methods for Viscosity Solutions and Applications CY SEP 06-08, 2004 CL Univ Roma La Sapienza, Dipartimento Matemat, Rome, ITALY HO Univ Roma La Sapienza, Dipartimento Matemat DE Hamilton-Jacobi equations; central schemes; semi-discrete schemes; high order; WENO; weighted power ENO; mapped ENO ID ESSENTIALLY NONOSCILLATORY SCHEMES; CENTRAL-UPWIND SCHEMES; VISCOSITY SOLUTIONS; CONSERVATION-LAWS; TRIANGULAR MESHES; DISCRETIZATION AB We incorporate new high-order WENO-type reconstructions into Godunov-type central schemes for Hamilton-Jacobi equations. We study schemes that are obtained by combining the Kurganov-Noelle-Petrova flux with the weighted power ENO and the mapped WENO reconstructions. We also derive new variants of these reconstructions by composing the weighted power ENO and the mapped WENO reconstructions with each other. While all schemes are, formally, fifth-order accurate, we show that the quality of the approximation does depend on the particular reconstruction that is being used. In certain cases, it is shown that the approximate solution may not converge to the viscosity solution at all. (c) 2006 IMACS. Published by Elsevier B.V. All rights reserved. C1 NASA, Ames Res Ctr, Adv Supercomp Div, Moffett Field, CA 94035 USA. Stanford Univ, Dept Math, Stanford, CA 94305 USA. RP Bryson, S (reprint author), NASA, Ames Res Ctr, Adv Supercomp Div, Moffett Field, CA 94035 USA. EM sbryson@mail.arc.nasa.gov; dlevy@math.stanford.edu NR 29 TC 12 Z9 12 U1 0 U2 4 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0168-9274 EI 1873-5460 J9 APPL NUMER MATH JI Appl. Numer. Math. PD SEP PY 2006 VL 56 IS 9 BP 1211 EP 1224 DI 10.1016/j.apnum.2006.03.005 PG 14 WC Mathematics, Applied SC Mathematics GA 066ZC UT WOS:000239268400007 ER PT J AU Abdeldayem, HA Dowdye, E Canham, J AF Abdeldayem, H. A. Dowdye, E. Canham, J. TI Roles of contamination and nonlinear effects in failing space-flight lasers SO APPLIED PHYSICS B-LASERS AND OPTICS LA English DT Article ID INDUCED OPTICAL-DAMAGE; BEAM; ATOMS AB Space-flight lasers are subjected to a harsh space environment that affects their performances and lifetimes. Contamination and induced nonlinear optical effects are the most worrisome factors that frequently contribute to laser failure in space. In this paper, we present a descriptive physical model that explains the cause of surface damage of optical components due to contamination, nonlinear phenomena, and the role of microgravity and the optical forces in the process. Experimental results are presented and discussed. An adsorption technique to minimize the presence of contaminants is proposed. C1 NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Swales Aerosp Inc, Beltsville, MD 20705 USA. RP Abdeldayem, HA (reprint author), NASA, Goddard Space Flight Ctr, Code 554, Greenbelt, MD 20771 USA. EM hossin.abdeldayem@nasa.gov NR 18 TC 0 Z9 0 U1 3 U2 7 PU SPRINGER PI NEW YORK PA 233 SPRING STREET, NEW YORK, NY 10013 USA SN 0946-2171 J9 APPL PHYS B-LASERS O JI Appl. Phys. B-Lasers Opt. PD SEP PY 2006 VL 84 IS 3 BP 447 EP 452 DI 10.1007/s00340-006-2242-x PG 6 WC Optics; Physics, Applied SC Optics; Physics GA 068SH UT WOS:000239394200014 ER PT J AU Yu, N Kohel, JM Kellogg, JR Maleki, L AF Yu, N. Kohel, J. M. Kellogg, J. R. Maleki, L. TI Development of an atom-interferometer gravity gradiometer for gravity measurement from space SO APPLIED PHYSICS B-LASERS AND OPTICS LA English DT Article ID STIMULATED RAMAN TRANSITIONS; CLOCK AB Recent progress in cold atom interferometry has lead to a new method of sensitive inertial sensing. Significant performance enhancement of cold atom interferometer-based sensors is anticipated when operated in the microgravity environment in space. Based on cold atom interferometer techniques, we are developing a quantum gravity gradiometer for satellite-based global gravity field mapping. As a first step, we have built a laboratory-based gradiometer employing component technologies suitable for a future flight instrument. This paper describes the implementation of the laboratory instrument and its initial results. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Yu, N (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM nan.yu@jpl.nasa.gov NR 21 TC 51 Z9 53 U1 3 U2 14 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0946-2171 J9 APPL PHYS B-LASERS O JI Appl. Phys. B-Lasers Opt. PD SEP PY 2006 VL 84 IS 4 BP 647 EP 652 DI 10.1007/s00340-006-2376-x PG 6 WC Optics; Physics, Applied SC Optics; Physics GA 082BK UT WOS:000240361300014 ER PT J AU Stirling, I Parkinson, CL AF Stirling, Ian Parkinson, Claire L. TI Possible effects of climate warming on selected populations of polar bears (Ursus maritimus) in the Canadian Arctic SO ARCTIC LA English DT Article DE climate warming; polar bear; Ursus maritimus; sea ice; Arctic ID WESTERN HUDSON-BAY; SEA-ICE COVER; PHOCA-HISPIDA; HOODED SEALS; RINGED SEALS; REPRODUCTIVE SUCCESS; CYSTOPHORA-CRISTATA; DAVIS STRAIT; TIME-SERIES; TRENDS AB Polar bears depend on sea ice for survival. Climate warming in the Arctic has caused significant declines in total cover and thickness of sea ice in the polar basin and progressively earlier breakup in some areas. Inuit hunters in the areas of four polar bear populations in the eastern Canadian Arctic (including Western Hudson Bay) have reported seeing more bears near settlements during the open-water period in recent years. In a fifth ecologically similar population, no changes have yet been reported by Inuit hunters. These observations, interpreted as evidence of increasing population size, have resulted in increases in hunting quotas. However, long-term data on the population size and body condition of polar bears in Western Hudson Bay, as well as population and harvest data from Baffin Bay, make it clear that those two populations at least are more likely to be declining, not increasing. While the ecological details vary in the regions occupied by the five different populations discussed in this paper, analysis of passive-microwave satellite imagery beginning in the late 1970s indicates that the sea ice is breaking up at progressively earlier dates, so that bears must fast for longer periods during the open-water season. Thus, at least part of the explanation for the appearance of more bears near coastal communities and hunting camps is likely that they are searching for alternative food sources in years when their stored body fat depots may be depleted before freeze-up, when they can return to the sea ice to hunt seals again. We hypothesize that, if the climate continues to warm as projected by the Intergovernmental Panel on Climate Change (IPCC), then polar bears in all five populations discussed in this paper will be increasingly food-stressed, and their numbers are likely to decline eventually, probably significantly so. As these populations decline, problem interactions between bears and humans will likely continue, and possibly increase, as the bears seek alternative food sources. Taken together, the data reported in this paper suggest that a precautionary approach be taken to the harvesting of polar bears and that the potential effects of climate warming be incorporated into planning for the management and conservation of this species throughout the Arctic. C1 Canadian Wildlife Serv, Edmonton, AB T6H 3S5, Canada. NASA, Goddard Space Flight Ctr, Cryospher Sci Branch, Greenbelt, MD 20771 USA. RP Stirling, I (reprint author), Canadian Wildlife Serv, 5320 122 St, Edmonton, AB T6H 3S5, Canada. EM ian.stirling@ec.gc.ca RI Parkinson, Claire/E-1747-2012 OI Parkinson, Claire/0000-0001-6730-4197 NR 75 TC 165 Z9 174 U1 25 U2 263 PU ARCTIC INST N AMER PI CALGARY PA UNIV OF CALGARY 2500 UNIVERSITY DRIVE NW 11TH FLOOR LIBRARY TOWER, CALGARY, ALBERTA T2N 1N4, CANADA SN 0004-0843 J9 ARCTIC JI Arctic PD SEP PY 2006 VL 59 IS 3 BP 261 EP 275 PG 15 WC Environmental Sciences; Geography, Physical SC Environmental Sciences & Ecology; Physical Geography GA 092UI UT WOS:000241122400004 ER PT J AU Corwin, TM Sumerel, AN Pritzl, BJ Smith, HA Catelan, M Sweigart, AV Stetson, PB AF Corwin, T. Michael Sumerel, Andrew N. Pritzl, Barton J. Smith, Horace A. Catelan, M. Sweigart, Allen V. Stetson, Peter B. TI Image-subtraction photometry of variable stars in the globular clusters NGC 6388 and NGC 6441 SO ASTRONOMICAL JOURNAL LA English DT Article DE globular clusters : individual ( NGC 6441NGC 6388); stars : evolution; stars : variables : other ID RR-LYRAE VARIABLES; BLUE HORIZONTAL-BRANCH; METAL-RICH; NGC 6441; DISCOVERY; CATALOG; NGC-6791; PLANETS; SEARCH AB We have applied Alard's image-subtraction method (ISIS ver. 2.1) to the observations of the globular clusters NGC 6388 and NGC 6441 previously analyzed using standard photometric techniques (DAOPHOT and ALLFRAME). In this reanalysis of observations obtained at the Cerro Tololo Inter-American Observatory, besides recovering the variables previously detected on the basis of our ground-based images, we have also been able to recover most of the RR Lyrae variables previously detected only in the analysis of Hubble Space Telescope WFPC2 observations of the inner region of NGC 6441. In addition, we report five possible new variables not found in the analysis of the Hubble Space Telescope observations of NGC 6441. This dramatically illustrates the capabilities of image-subtraction techniques applied to ground-based data to recover variables in extremely crowded fields. We have also detected 12 new variables and 6 possible variables in NGC 6388 not found in our previous ground-based studies. The revised mean period for RRab stars in NGC 6388 is 0.676 days, while the mean period of RRab stars in NGC 6441 is unchanged at 0.759 days. These values are among the largest known for any Galactic globular cluster. Additional probable type II Cepheids were identified in NGC 6388, confirming its status as a metal-rich globular cluster rich in Cepheids. C1 Univ N Carolina, Dept Phys & Opt Sci, Charlotte, NC 28223 USA. Macalester Coll, Dept Phys & Astron, St Paul, MN 55105 USA. Michigan State Univ, Dept Phys & Astron, E Lansing, MI 48824 USA. Pontificia Univ Catolica Chile, Dept Astron & Astrophys, Santiago 7820436, Chile. NASA Goddard Space Flight Ctr, Exploar Universe Div, Greenbelt, MD 20771 USA. Natl Res Council Canada, Herzberg Inst Astrophys, Doninion Astrophys Observ, Victoria, BC V9E 2E7, Canada. RP Corwin, TM (reprint author), Univ N Carolina, Dept Phys & Opt Sci, Charlotte, NC 28223 USA. EM mcorwin@uncc.edu; ansumere@uncc.edu; pritzl@macalester.edu; smith@pa.msu.edu; mcatelan@astro.puc.cl; sweigart@bach.gsfc.nasa.gov; peter.stetson@nrc-cnrc.gc.ca NR 34 TC 21 Z9 21 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-6256 J9 ASTRON J JI Astron. J. PD SEP PY 2006 VL 132 IS 3 BP 1014 EP 1022 DI 10.1086/505745 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 082RA UT WOS:000240403700006 ER PT J AU Wadadekar, Y Casertano, S De Mello, D AF Wadadekar, Yogesh Casertano, Stefano De Mello, Duilia TI Faint U-band dropouts in the WFPC2 parallels of the Hubble Ultra Deep Field SO ASTRONOMICAL JOURNAL LA English DT Article DE cosmology : observations; galaxies : distances and redshifts; galaxies : evolution; galaxies : statistics; ultraviolet : galaxies ID LYMAN-BREAK GALAXIES; HIGH-REDSHIFT GALAXIES; STAR-FORMATION HISTORY; ULTRAVIOLET LUMINOSITY; STELLAR POPULATIONS; EVOLUTION; MORPHOLOGIES; Z-SIMILAR-TO-2; SELECTION; UNIVERSE AB We combine data from the extremely deep Hubble Space Telescope U (F300W) image, obtained using WFPC2 as part of the parallel observations of the Hubble Ultra Deep Field campaign, with BVi images from the Great Observatories Origins Deep Survey to identify a sample of Lyman break galaxies in the redshift range 2.0 less than or similar to z less than or similar to 3.5. We use recent stellar population synthesis models with a wide variety of ages, metallicities, redshifts, and dust content, and a detailed representation of the H I cosmic opacity as a function of redshift to model the colors of galaxies in our combination of WFPC2 and ACS filters. Using these models, we derive improved color selection criteria that provide a clean selection of relatively unobscured star- forming galaxies in this redshift range. Our WFPC2 F300W image is the deepest image ever obtained at that wavelength. The 10 sigma limiting magnitude measured over 0.2 arcsec(2) is 27.5 mag in the WFPC2 F300W image, about 0.5 mag deeper than the F300W image in the Hubble Deep Field ( HDF) - North. This extra depth relative to the HDFs allows us to directly probe the luminosity function about 0.5 mag deeper than the depth accessible with the HDF data along an independent line of sight. Our sample of star- forming galaxies with 2.0 less than or similar to z less than or similar to 3.5 includes 125 objects, the majority of which show clumpy morphologies. We measure a star formation rate density of 0.18 M circle dot yr(-1) Mpc(-3), marginally higher than the value measured for the HDFs. C1 Space Telescope Sci Inst, Baltimore, MD 21218 USA. Goddard Space Flight Ctr, Observ Cosmol Lab, Greenbelt, MD 20771 USA. Catholic Univ America, Dept Phys, Washington, DC 20064 USA. Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. RP Wadadekar, Y (reprint author), Space Telescope Sci Inst, 3700 San Martin Dr, Baltimore, MD 21218 USA. NR 52 TC 7 Z9 7 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-6256 J9 ASTRON J JI Astron. J. PD SEP PY 2006 VL 132 IS 3 BP 1023 EP 1034 DI 10.1086/505747 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 082RA UT WOS:000240403700007 ER PT J AU Carson, JC Eikenberry, SS Smith, JJ Cordes, JM AF Carson, J. C. Eikenberry, S. S. Smith, J. J. Cordes, J. M. TI The Cornell High-Order Adaptive Optics Survey for brown dwarfs in stellar systems. II. Results from Monte Carlo population analyses SO ASTRONOMICAL JOURNAL LA English DT Article DE methods : numerical; methods : statistical; stars : low mass, brown dwarfs; surveys ID SUBSTELLAR MASS FUNCTION; SOLAR NEIGHBORHOOD; STAR-FORMATION; COMPANIONS; CLUSTER; SAMPLE; MULTIPLICITY; PLANETS; AGE AB In this second of a two-paper sequence, we present Monte Carlo population simulation results of brown dwarf companion data collected during the Cornell High-Order Adaptive Optics Survey (CHAOS) for brown dwarf companions. Making reasonable assumptions of orbital parameters (random inclination, random eccentricity, and random longitude of pericenter) and age distributions and using published mass functions, we find that the brown dwarf companion fraction around main-sequence stars is 0.0%-9.3% for the 25-100 AU semimajor axis region. We find a corresponding L dwarf companion fraction of 0.0%-3.3%. We compare our population analysis methods and results with techniques and results presented by several other groups. In this comparison we discover that systematic errors (most notably resulting from orbital projection effects) occur in the majority of previously published brown dwarf companion population estimates, leading authors to claim results not supported by the observational data. C1 Cornell Univ, Dept Astron, Ithaca, NY 14853 USA. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. Cornell Univ, Dept Astron, Ithaca, NY 14853 USA. RP Carson, JC (reprint author), Cornell Univ, Dept Astron, Ithaca, NY 14853 USA. NR 31 TC 19 Z9 19 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 SEP PY 2006 VL 132 IS 3 BP 1146 EP 1152 DI 10.1086/505705 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 082RA UT WOS:000240403700015 ER PT J AU Gomez, JF De Gregorio-Monsalvo, I Suarez, O Kuiper, TBH AF Gomez, Jose F. De Gregorio-Monsalvo, Itziar Suarez, Olga Kuiper, Thomas B. H. TI A sensitive survey for water maser emission toward Bok globules using the Robledo 70m antenna SO ASTRONOMICAL JOURNAL LA English DT Article DE ISM : globules; masers; radio lines : ISM; stars : formation; stars : pre-main-sequence ID YOUNG STELLAR OBJECTS; STAR-FORMING REGIONS; HERBIG-HARO OBJECTS; SPECTRAL ENERGY-DISTRIBUTIONS; OPHIUCHI INFRARED CLUSTER; RADIO-CONTINUUM EMISSION; SMALL DARK CLOUDS; DENSE CORES; H2O MASERS; PROTOSTELLAR COLLAPSE AB We report on the most sensitive water maser survey toward Bok globules to date, performed using NASA's 70 m antenna at Robledo de Chavela (Spain). We observed 207 positions within the Clemens and Barvainis catalog with a higher probability of harboring a young star, using as selection criteria the presence of radio continuum emission (from submillimeter to centimeter wavelengths), geometric centers of molecular outflows, peaks in maps of high-density gas tracers (NH3 or CS), and IRAS point sources. We have obtained seven maser detections, six of which (in CB 34, CB 54, CB 65, CB 101, CB 199, and CB 232) are reported for the first time here. Most of the water masers we detected are likely to be associated with young stellar objects (YSOs), except for CB 101 (probably an evolved object) and CB 65 (uncertain nature). The water maser in CB 199 shows a relatively high shift (similar or equal to 30 km s(-1)) of its velocity centroid with respect to the cloud velocity, which is unusual for low-mass YSOs. We speculate that high-velocity masers in this kind of object could be related to episodes of energetic mass loss in close binaries. Alternatively, the maser in CB 199 could be pumped by a protoplanetary or a young planetary nebula. CB 232 is the smallest Bok globule (similar or equal to 0.6 pc) known to be associated with water maser emission, although it would be superseded by the cases of CB 65 (similar or equal to 0.3 pc) and CB 199 (similar or equal to 0.5 pc) if their association with YSOs is confirmed. All our selection criteria have statistically compatible detection rates, except for IRAS sources, which tend to be somewhat worse predictors for the presence of maser emission. C1 CSIC, Inst Astrofis Andalucia, E-18080 Granada, Spain. INTA, Lab Astrofis Espacial & Fis Fundamental, E-28080 Madrid, Spain. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Gomez, JF (reprint author), CSIC, Inst Astrofis Andalucia, Apartado 3004, E-18080 Granada, Spain. EM jfg@iaa.es; itziar@laeff.inta.es; olga@laeff.inta.es RI Gomez, Jose Francisco/D-8392-2016 OI Gomez, Jose Francisco/0000-0002-7065-542X NR 87 TC 14 Z9 14 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-6256 J9 ASTRON J JI Astron. J. PD SEP PY 2006 VL 132 IS 3 BP 1322 EP 1332 DI 10.1086/506514 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 082RA UT WOS:000240403700030 ER PT J AU Tennant, AF AF Tennant, Allyn F. TI Chandra observation of NGC 6822 SO ASTRONOMICAL JOURNAL LA English DT Article DE galaxies : individual ( NGC 6822); methods : data analysis; X-rays : galaxies ID X-RAY OBSERVATIONS; GALAXY NGC-6822; POINT-SOURCE; CATALOG; STAR AB Chandra observed the nearby dwarf galaxy NGC 6822. There are 70 sources in the Chandra field, two of which are fairly extended and likely background clusters of galaxies. A third source was resolved by Chandra that has the same size and position as a known supernova remnant. The suspected variability detected from this source in previous missions is shown to be in error. The majority of the remaining 67 sources are consistent with background sources. Of the 61 sources detected above a completeness limit of 10 events, we estimate that 9 +/- 4 +/- 8 are associated with the galaxy, including both systematic and statistical errors. We compare the X-ray positions of all sources with various catalogs and Hubble Space Telescope data and offer tentative identifications for several. Based on the mass and star formation rate of NGC 6822, we expect only about 10 sources, mostly high-mass systems. C1 NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA. RP Tennant, AF (reprint author), NASA, George C Marshall Space Flight Ctr, VP 62, Huntsville, AL 35812 USA. EM allyn.tennant@msfc.nasa.gov NR 21 TC 21 Z9 21 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-6256 J9 ASTRON J JI Astron. J. PD SEP PY 2006 VL 132 IS 3 BP 1372 EP 1383 DI 10.1086/506511 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 082RA UT WOS:000240403700035 ER PT J AU Hendrix, AR Vilas, F AF Hendrix, Amanda R. Vilas, Faith TI The effects of space weathering at UV wavelengths: S-class asteroids SO ASTRONOMICAL JOURNAL LA English DT Article DE minor planets, asteroids; Moon; ultraviolet : solar system ID NEAR-EARTH ASTEROIDS; ION IRRADIATION EXPERIMENTS; MAIN-BELT; SPECTROSCOPIC SURVEY; SPECTRAL PROPERTIES; REFLECTANCE SPECTRA; ORDINARY CHONDRITES; LUNAR; REGOLITH; SIMULATION AB We present evidence that space weathering manifests itself at near-UV wavelengths as a bluing of the spectrum, in contrast with the spectral reddening that has been seen at visible-near-IR wavelengths. Furthermore, the effects of space weathering at UV wavelengths tend to appear with less weathering than do the longer wavelength effects, suggesting that the UV wavelength range is a more sensitive indicator of weathering, and thus age. We report results from analysis of existing near-UV (similar to 220-350 nm) measurements of S-type asteroids from the International Ultraviolet Explorer and the Hubble Space Telescope and comparisons with laboratory measurements of meteorites to support this hypothesis. Composite spectra of S asteroids are produced by combining UV spacecraft data with ground-based longer wavelength data. At visible-near-IR wavelengths, S-type asteroids are generally spectrally redder (and darker) than ordinary chondrite meteorites, whereas the opposite is generally true at near-UV wavelengths. Similarly, laboratory measurements of lunar samples show that lunar soils (presumably more weathered) are spectrally redder at longer wavelengths, and spectrally bluer at near-UV wavelengths, than less weathered crushed lunar rocks. The UV spectral bluing may be a result of the addition of nanophase iron to the regolith through the weathering process. The UV bluing is most prominent in the 300-400 nm range, where the strong UV absorption edge is degraded with weathering. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. NASA, Lyndon B Johnson Space Ctr, Planetary Astron Grp, Houston, TX 77058 USA. RP Hendrix, AR (reprint author), CALTECH, Jet Prop Lab, MS 230-250, Pasadena, CA 91109 USA. EM arh@jpl.nasa.gov NR 52 TC 28 Z9 28 U1 0 U2 5 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-6256 J9 ASTRON J JI Astron. J. PD SEP PY 2006 VL 132 IS 3 BP 1396 EP 1404 DI 10.1086/506426 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 082RA UT WOS:000240403700037 ER PT J AU Stern, D Chary, RR Eisenhardt, PRM Moustakas, LA AF Stern, Daniel Chary, Ranga-Ram Eisenhardt, Peter R. M. Moustakas, Leonidas A. TI Spitzer observations of the prototypical extremely red objects HR 10 and LBDS 53W091: Separating dusty starbursts from old elliptical galaxies SO ASTRONOMICAL JOURNAL LA English DT Article DE galaxies : evolution; galaxies : individual (HR 10, LBDS 53W069, LBDS 53W091); infrared : galaxies ID HUBBLE-DEEP-FIELD; STAR-FORMATION HISTORIES; STELLAR MASS DENSITY; DIGITAL SKY SURVEY; HIGH-REDSHIFT; RADIO GALAXIES; SPACE-TELESCOPE; K20 SURVEY; LUMINOSITY; EVOLUTION AB We present Spitzer Space Telescope observations of the well-studied extremely red objects (EROs) HR 10 and LBDS 53W091 from 3.6 to 160 mu m. These galaxies are the prototypes of the two primary classes of EROs: dusty starbursts and old, evolved galaxies, respectively. Both galaxies, as well as LBDS 53W069, another example of an old, quiescent galaxy, are well detected out to 8 mu m. However, only the dusty starburst HR 10 is detected in the far-infrared. All three EROs have stellar masses of a few x 10(11) M-circle dot. Using evolutionary model fits to their multiband photometry, we predict the infrared colors of similar EROs at 1 < z < 2. We find that blueward of observed 10 mu m, the two ERO classes are virtually indistinguishable photometrically. Deep spectroscopy and 24 mu m data allow the classes to be separated. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA. RP Stern, D (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. EM stern@zwolfkinder.jpl.nasa.gov OI Moustakas, Leonidas/0000-0003-3030-2360 NR 70 TC 25 Z9 25 U1 0 U2 3 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-6256 J9 ASTRON J JI Astron. J. PD SEP PY 2006 VL 132 IS 3 BP 1405 EP 1414 DI 10.1086/506347 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 082RA UT WOS:000240403700038 ER PT J AU Tang, SM Zhang, SN AF Tang, S. M. Zhang, S. N. TI Time lag between prompt optical emission and gamma-rays in GRBs (Research Note) SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE gamma rays : bursts; methods : data analysis ID BURST; AFTERGLOW AB Aims. The prompt optical emission contemporaneous with the gamma-rays from gamma-ray bursts (GRBs) carries important information on the central engine and explosion mechanism. We study the time lag between prompt optical emission and gamma-rays in GRB 990123 and GRB 041219a, which are the only two GRBs detected at optical wavelengths during the ascending burst phase. Methods. Assuming profiles of prompt optical light curves are the same as the prompt gamma-rays, we simulate optical light curves with different time lags and compare them with the observed optical flux. Then the best fit time lag and its error are determined by chi-squared values. Results. We find that time lags between prompt optical emission and gamma-rays in GRB host galaxy rest-frames are consistent in the two GRBs, which is 5 similar to 7 s for GRB 990123 and 1 similar to 5 s for GRB 041219a. This result is consistent with a common origin of prompt optical and gamma-ray emissions in the two GRBs. Based on synchrotron cooling model, we also derive the parameters for the two GRBs. C1 Tsing Hua Univ, Dept Phys, Beijing 100084, Peoples R China. Tsing Hua Univ, Ctr Astrophys, Beijing 100084, Peoples R China. Univ Alabama, Dept Phys, Huntsville, AL 35899 USA. NASA, George C Marshall Space Flight Ctr, Space Sci Lab, Huntsville, AL 35812 USA. Chinese Acad Sci, Inst High Energy Phys, Beijing 100039, Peoples R China. RP Tang, SM (reprint author), Tsing Hua Univ, Dept Phys, Beijing 100084, Peoples R China. EM tangsm99@mails.tsinghua.edu.cn 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 SEP PY 2006 VL 456 IS 1 BP 141 EP 143 DI 10.1051/0004-6361:20065547 PG 3 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 077EE UT WOS:000240009800013 ER PT J AU Cotton, WD Vlemmings, W Mennesson, B Perrin, G du Foresto, VC Chagnon, G Diamond, PJ van Langevelde, HJ Bakker, E Ridgway, S Mc Allister, H Traub, W Ragland, S AF Cotton, W. D. Vlemmings, W. Mennesson, B. Perrin, G. du Foresto, V. Coude Chagnon, G. Diamond, P. J. van Langevelde, H. J. Bakker, E. Ridgway, S. Mc Allister, H. Traub, W. Ragland, S. TI Further VLBA observations of SiO masers toward Mira variable stars SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE stars : atmospheres; stars : AGB and post-AGB; stars : variables : general; radio lines : stars; masers ID LINEARLY POLARIZED RADIATION; ASTROPHYSICAL MASERS; MAGNETIC-FIELDS; R-AQUARII; CIRCULAR-POLARIZATION; TX CAM; EMISSION; VARIABILITY; PERIOD; GHZ AB We present the results of continued monitoring of the SiO masers at 7 mm wavelength in several of the Mira variable stars reported in Cotton et al. (2004, A&A, 414, 275) (o Ceti = Mira, U Orionis = U Ori, R Aquarii = R Aqr) over a period of 16 months, extending the observations to several pulsation cycles. The observed size of the maser rings varied by 3-14% with time but show no clear correlation with pulsation phase. In all cases, the SiO masers appear just outside the dense molecular layer indicated by near-IR observations. Rotation (or large scale motion) is possibly detected in o Ceti with a period of 89 x sin(i) years. We find linear polarization up to similar to 60% and at several epochs predominantly tangentially ordered polarization vectors indicate a radial magnetic field direction. Jet-like features are examined in o Ceti and R Aqr and in both cases, the magnetic field appears elongated with the masing structure. This suggests that the dynamic feature in the envelope is dragging the magnetic field or that the gas is constrained to follow magnetic field. C1 Natl Radio Astron Observ, Charlottesville, VA 22903 USA. Univ Manchester, Jodrell Bank Observ, Macclesfield SK11 9DL, Cheshire, England. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. Observ Paris, DESPA, F-92190 Meudon, France. Joint Inst VLIB Europe, NL-7990 AA Dwingeloo, Netherlands. Natl Opt Astron Observ, Tucson, AZ 85726 USA. Leiden Observ, NL-2300 RA Leiden, Netherlands. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Georgia State Univ, Atlanta, GA 30303 USA. WM Keck Observ, Kamuela, HI 96743 USA. RP Cotton, WD (reprint author), Natl Radio Astron Observ, 520 Edgemont Rd, Charlottesville, VA 22903 USA. EM bcotton@nrao.edu OI van Langevelde, Huib Jan/0000-0002-0230-5946; /0000-0002-2700-9916 NR 32 TC 35 Z9 35 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 SEP PY 2006 VL 456 IS 1 BP 339 EP U70 DI 10.1051/0004-6361:20065134 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 077EE UT WOS:000240009800035 ER PT J AU Antonelli, LA Testa, V Romano, P Guetta, D Torii, K D'Elia, V Malesani, D Chincarini, G Covino, S D'Avanzo, P Della Valle, M Fiore, F Fugazza, D Moretti, A Stella, L Tagliaferri, G Barthelmy, S Burrows, D Campana, S Capalbi, M Cusumano, G Gehrels, N Giommi, P Lazzati, D La Parola, V Mangano, V Mineo, T Nousek, J O'Brien, PT Perri, M AF Antonelli, L. A. Testa, V. Romano, P. Guetta, D. Torii, K. D'Elia, V. Malesani, D. Chincarini, G. Covino, S. D'Avanzo, P. Della Valle, M. Fiore, F. Fugazza, D. Moretti, A. Stella, L. Tagliaferri, G. Barthelmy, S. Burrows, D. Campana, S. Capalbi, M. Cusumano, G. Gehrels, N. Giommi, P. Lazzati, D. La Parola, V. Mangano, V. Mineo, T. Nousek, J. O'Brien, P. T. Perri, M. TI The multiwavelength afterglow of GRB 050721: a puzzling rebrightening seen in the optical but not in the X-ray SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE gamma ray : bursts ID BURST; TELESCOPE; SUPERNOVA; EMISSION; GRB-030329; MISSION; LIGHT AB Context. GRB050721 was detected by Swift and promptly followed-up, in the X-ray by Swift itself and, in the optical band, by the VLT operated, for the first time, in rapid response mode starting observations about 25 m after the burst. A multiwavelength monitoring campaign was performed in order to study its afterglow's behavior. Aims. We present the analysis of the early and late afterglow emission in both the X-ray and optical bands, as observed by Swift, a robotic telescope, and the VLT. We compare early observations with late afterglow observations obtained with Swift and the VLT in different bands in order to constrain the density of the medium in which the fireball is expanding. Methods. We have analyzed both the X-ray and the optical light curves and compared the spectral energy distribution of the afterglow at two different epochs. Results. We observed an intense rebrightening in the optical band at about one day after the burst which was not seen in the X-ray band. This is the first observation of a GRB afterglow in which a rebrightening is observed in the optical but not in the X-ray band. The lack of detection in X-ray of such a strong rebrightening at lower energies may be described with a variable external density profile. In such a scenario, the combined X-ray and optical observations allow us to derive that matter located at similar to 10(17) cm from the burst is about a factor of 10 higher than in the inner region. C1 INAF Astron Observ Rome, I-00040 Rome, Italy. ASI Sci Data Ctr, I-00044 Rome, Italy. ASI Sci Data Ctr, I-23807 Merate, Italy. INAF Astron Observ Brera, I-23807 Merate, Italy. Osaka Univ, Grad Sch Sci, Dept Earth & Space Sci, Toyonaka, Osaka 5600043, Japan. SISSA ISAS, I-34014 Trieste, Italy. Univ Milan, I-20126 Milan, Italy. INAF Astrophys Observ Arcetri, I-50125 Florence, Italy. Univ Calif Santa Barbara, Kavli Inst Theoret Phys, Santa Barbara, CA 93106 USA. NASA Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. INAF, Sez Palermo, I-90146 Palermo, Italy. Univ Colorado, JILA, Boulder, CO 80309 USA. Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England. RP Antonelli, LA (reprint author), INAF Astron Observ Rome, Via Frascati 33, I-00040 Rome, Italy. EM a.antonelli@oa-roma.inaf.it RI Barthelmy, Scott/D-2943-2012; Gehrels, Neil/D-2971-2012; OI D'Elia, Valerio/0000-0002-7320-5862; Cusumano, Giancarlo/0000-0002-8151-1990; moretti, alberto/0000-0002-9770-0315; Della Valle, Massimo/0000-0003-3142-5020; Perri, Matteo/0000-0003-3613-4409; La Parola, Valentina/0000-0002-8087-6488; Mineo, Teresa/0000-0002-4931-8445; guetta, dafne/0000-0002-7349-1109; giommi, paolo/0000-0002-2265-5003; Covino, Stefano/0000-0001-9078-5507; Tagliaferri, Gianpiero/0000-0003-0121-0723; Testa, Vincenzo/0000-0003-1033-1340; Fiore, Fabrizio/0000-0002-4031-4157 NR 48 TC 15 Z9 15 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 SEP PY 2006 VL 456 IS 2 BP 509 EP 515 DI 10.1051/0004-6361:20065283 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 080IZ UT WOS:000240242400012 ER PT J AU Giommi, P Blustin, AJ Capalbi, M Colafrancesco, S Cucchiara, A Fuhrmann, L Krimm, HA Marchili, N Massaro, E Perri, M Tagliaferri, G Tosti, G Tramacere, A Burrows, DN Chincarini, G Falcone, A Gehrels, N Kennea, J Sambruna, R AF Giommi, P. Blustin, A. J. Capalbi, M. Colafrancesco, S. Cucchiara, A. Fuhrmann, L. Krimm, H. A. Marchili, N. Massaro, E. Perri, M. Tagliaferri, G. Tosti, G. Tramacere, A. Burrows, D. N. Chincarini, G. Falcone, A. Gehrels, N. Kennea, J. Sambruna, R. TI Swift and infra-red observations of the blazar 3C 454.3 during the giant X-ray flare of May 2005 SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE radiation mechanisms : non-thermal; galaxies : active; galaxies : quasars : individual : 3C 454.3 ID EMISSION; REM; TELESCOPE; QUASARS; RADIATION; OUTBURST; CTA-102; MISSION; STARS AB We present the results of a series of Swift and quasi simultaneous ground-based infra-red observations of the blazar 3C 454.3 carried out in April-May 2005 when the source was 10 to 30 times brighter than previously observed. We found 3C 454.3 to be very bright and variable at all frequencies covered by our instrumentation. The broad-band Spectral Energy Distribution (SED) shows the usual two-bump shape (in Log v -Log [vf(v)] space) with the Infra-red, optical and UV data sampling the declining part of the synchrotron emission that, even during this extremely large outburst, had its maximum in the far-infrared. The X-ray spectral data from the XRT and BAT instruments are flat and due to inverse Compton emission. The remarkable SED observed implies that at the time of the Swift pointings 3C 454.3 was one of the brightest objects in the extragalactic sky with gamma-ray emission similar or brighter than that of 3C 279 when observed in a high state by EGRET. Time variability in the optical-UV flux is very different from that in the X-ray data: while the first component varied by about a factor two within a single exposure, but remained approximately constant between different observations, the inverse Compton component did not vary on short time-scales but changed by more than a factor of 3 between observations separated by a few days. This different dynamical behaviour illustrates the need to collect simultaneous multi-frequency data over a wide range of time-scales to fully constrain physical parameters in blazars. C1 ASDC, ASI Sci Data Ctr, I-00044 Frascati, Italy. UCL, Mullard Space Sci Lab, Dorking RH5 6NT, Surrey, England. Osserv Astron Roma, INAF, I-00040 Monte Porzio Catone, Italy. Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. Univ Perugia, Dipartimento Fis, I-06100 Perugia, Italy. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Univ Roma La Sapienza, Dipartimento Fis, I-00185 Rome, Italy. Osserv Astron Brera, INAF, I-23807 Merate, Italy. RP Giommi, P (reprint author), ASDC, ASI Sci Data Ctr, Via G Galilei, I-00044 Frascati, Italy. EM paolo.giommi@asi.it RI Gehrels, Neil/D-2971-2012; Tosti, Gino/E-9976-2013; OI Perri, Matteo/0000-0003-3613-4409; Tramacere, Andrea/0000-0002-8186-3793; Tagliaferri, Gianpiero/0000-0003-0121-0723; giommi, paolo/0000-0002-2265-5003 NR 39 TC 62 Z9 62 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 SEP PY 2006 VL 456 IS 3 BP 911 EP 916 DI 10.1051/0004-6361:20064874 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 082ES UT WOS:000240370100010 ER PT J AU Romano, P Campana, S Chincarini, G Cummings, J Cusumano, G Holland, ST Mangano, V Mineo, T Page, KL Pal'shin, V Rol, E Sakamoto, T Zhang, B Aptekar, R Barbier, S Barthelmy, S Beardmore, AP Boyd, P Burrows, DN Capalbi, M Fenimore, EE Frederiks, D Gehrels, N Giommi, P Goad, MR Godet, O Golenetskii, S Guetta, D Kennea, JA La Parola, V Malesani, D Marshall, F Moretti, A Nousek, JA O'Brien, PT Osborne, JP Perri, M Tagliaferri, G AF Romano, P. Campana, S. Chincarini, G. Cummings, J. Cusumano, G. Holland, S. T. Mangano, V. Mineo, T. Page, K. L. Pal'shin, V. Rol, E. Sakamoto, T. Zhang, B. Aptekar, R. Barbier, S. Barthelmy, S. Beardmore, A. P. Boyd, P. Burrows, D. N. Capalbi, M. Fenimore, E. E. Frederiks, D. Gehrels, N. Giommi, P. Goad, M. R. Godet, O. Golenetskii, S. Guetta, D. Kennea, J. A. La Parola, V. Malesani, D. Marshall, F. Moretti, A. Nousek, J. A. O'Brien, P. T. Osborne, J. P. Perri, M. Tagliaferri, G. TI Panchromatic study of GRB 060124: from precursor to afterglow SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE gamma rays : bursts; X-rays : bursts; X-rays : individuals : GRB 060124 ID GAMMA-RAY BURST; OPTICAL FLASH; REVERSE SHOCK; LIGHT CURVES; BATSE OBSERVATIONS; ENGINE ACTIVITY; GRB 990123; EMISSION; SPECTRA; TELESCOPE AB We present observations of GRB 060124, the first event for which both the prompt and the afterglow emission could be observed simultaneously and in their entirety by the three Swift instruments. Indeed, Swift-BAT triggered on a precursor similar to 570 s before the main burst peak, and this allowed Swift to repoint the narrow field instruments to the burst position similar to 350 s before the main burst occurred. GRB 060124 also triggered Konus-Wind, which observed the prompt emission in a harder gamma-ray band (up to 2 MeV). Thanks to these exceptional circumstances, the temporal and spectral properties of the prompt emission can be studied in the optical, X-ray and gamma-ray ranges. While the X-ray emission (0.2-10 keV) clearly tracks the gamma-ray burst, the optical component follows a different pattern, likely indicating a different origin, possibly the onset of external shocks. The prompt GRB spectrum shows significant spectral evolution, with both the peak energy and the spectral index varying. As observed in several long GRBs, significant lags are measured between the hard-and low-energy components, showing that this behaviour extends over 3 decades in energy. The GRB peaks are also much broader at soft energies. This is related to the temporal evolution of the spectrum, and can be accounted for by assuming that the electron spectral index softened with time. The burst energy (E-iso similar to 5 x 10(53) erg) and average peak energy (E-p similar to 300 keV) make GRB 060124 consistent with the Amati relation. The X-ray afterglow is characterized by a decay which presents a break at t(b) similar to 10(5) s. C1 Osserv Astron Brera, INAF, Merate, LC, Italy. Univ Milan, I-20126 Milan, Italy. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. CNR, Washington, DC 20418 USA. Ist Astrofis Spaziale & Fis Cosm Sez Palermo, INAF, I-90146 Palermo, Italy. Univ Space Res Assoc, Columbia, MD 21044 USA. Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England. AF Ioffe Phys Tech Inst, St Petersburg 194021, Russia. Univ Nevada, Dept Phys, Las Vegas, NV 89154 USA. Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. ASI Sci Data Ctr, I-00044 Frascati, Italy. Los Alamos Natl Lab, Los Alamos, NM 87545 USA. Osserv Astron Roma, INAF, I-0040 Monte Porzio Catone, Italy. SISSA, ISAS, I-34014 Trieste, Italy. RP Romano, P (reprint author), Osserv Astron Brera, INAF, Via E Bianchi 46, Merate, LC, Italy. EM romano@merate.mi.astro.it RI Barthelmy, Scott/D-2943-2012; Boyd, Patricia/D-3274-2012; Gehrels, Neil/D-2971-2012; Frederiks, Dmitry/C-7612-2014; Pal'shin, Valentin/F-3973-2014; Aptekar, Raphail/B-3456-2015; Golenetskii, Sergey/B-3818-2015; OI Perri, Matteo/0000-0003-3613-4409; La Parola, Valentina/0000-0002-8087-6488; Tagliaferri, Gianpiero/0000-0003-0121-0723; Frederiks, Dmitry/0000-0002-1153-6340; Mineo, Teresa/0000-0002-4931-8445; guetta, dafne/0000-0002-7349-1109; giommi, paolo/0000-0002-2265-5003; Cusumano, Giancarlo/0000-0002-8151-1990; moretti, alberto/0000-0002-9770-0315 NR 89 TC 164 Z9 165 U1 0 U2 1 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD SEP PY 2006 VL 456 IS 3 BP 917 EP U30 DI 10.1051/0004-6361:20065071 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 082ES UT WOS:000240370100011 ER PT J AU Kadler, M Hughes, PA Ros, E Aller, MF Aller, HD AF Kadler, M. Hughes, P. A. Ros, E. Aller, M. F. Aller, H. D. TI A quasi-periodic modulation of the radio light curve of the blazar PKSB0048-097 SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE BL Lacertae objects : individual : PKSB0048-097; galaxies : active; galaxies : jets ID BL LACERTAE OBJECTS; ACTIVE GALACTIC NUCLEI; HELICAL JETS; VLBI SURVEY; SPACED DATA; AO 0235+16; VARIABILITY; BEHAVIOR; TIME AB In this letter we present the results of a wavelet analysis of the radio light curve of the BL Lac Object PKSB0048-097 from the University of Michigan Radio Astronomy Observatory monitoring program at 8 GHz during twenty-five years, from 1979 to 2004. The results show a remarkable periodicity of 450-470 days in the early 1980s that changed to a similar to 585 day periodicity in the late 1980s to early 1990s. A less pronounced similar to 400 day periodicity is found after similar to 1995. Very-long-baseline interferometry imaging at 15 GHz shows dramatic structural changes in the usually unresolved source between two epochs, 1995.57 and 2002.38. The pronounced northward directed jet seen in the 2002 image differs by more than 90 degrees in direction from the source structure found in earlier epochs. These findings make PKS B0048-097 a primary target for multi-wavelength observations and intensive radio monitoring to decipher the blazar-variability phenomenon. C1 Max Planck Inst Radioastron, D-53121 Bonn, Germany. NASA, Goddard Space Flight Ctr, Explorat Univ Div, Greenbelt, MD 20771 USA. Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. RP Kadler, M (reprint author), Max Planck Inst Radioastron, Auf Hugel 69, D-53121 Bonn, Germany. EM mkadler@milkyway.gsfc.nasa.gov; phughes@umich.edu; ros@mpifr-bonn.mpg.de; mfa@umich.edu; haller@umich.edu NR 20 TC 7 Z9 7 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 SEP PY 2006 VL 456 IS 2 BP L1 EP L4 DI 10.1051/0004-6361:200600026 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 080IZ UT WOS:000240242400041 ER PT J AU Mehlert, D Tapken, C Appenzeller, I Noll, S de Mello, D Heckman, TM AF Mehlert, D. Tapken, C. Appenzeller, I. Noll, S. de Mello, D. Heckman, T. M. TI Medium-resolution spectroscopy of galaxies with redshifts 2.3 < z < 3.5 SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE galaxies : high-redshift; galaxies : starburst; galaxies : abundances; galaxies : evolution ID STAR-FORMING GALAXIES; LYMAN-BREAK GALAXIES; FORS DEEP FIELD; MS 1512-CB58; METALLICITY DIAGNOSTICS; ULTRAVIOLET-SPECTRA; K20 SURVEY; EVOLUTION; Z-SIMILAR-TO-3; POPULATIONS AB Using FORS2 at the ESO VLT we obtained medium-resolution (R approximate to 2000) spectra of 12 galaxies with 2.37 <= z <= 3.40 in the FORS Deep Field. Two individual spectra with good S/N and a composite of all 12 spectra were used to derive properties of the stellar and interstellar absorption lines of galaxies in this redshift range. Systematic differences between the individual spectra were found for the strength and profiles of the intrinsic interstellar lines. For eight spectra with sufficient S/N, we measured the "1370" and "1425" metallicity indices, from which we find for our sample that galaxies at z > 3 have lower mean metallicity than galaxies at 2.3 < z < 3. However uncertainties remain concerning the absolute calibration of the metallicity tracers in use for high-redshift galaxies. Additional modeling will be needed to resolve these uncertainties. C1 Max Planck Inst Astron, D-67117 Heidelberg, Germany. Landessternwarte Heidelberg, D-69117 Heidelberg, Germany. MPE Garching, D-85748 Garching, Germany. NASA, Goddard Space Flight Ctr, Astron & Solar Phys Lab, Greenbelt, MD 20771 USA. Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA. Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. RP Mehlert, D (reprint author), Max Planck Inst Astron, Konigstuhl 17, D-67117 Heidelberg, Germany. EM tapken@mpia.de NR 42 TC 8 Z9 8 U1 0 U2 0 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD SEP PY 2006 VL 455 IS 3 BP 835 EP 843 DI 10.1051/0004-6361:20054066 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 074RN UT WOS:000239829600008 ER PT J AU Martin-Hernandez, NL Schaerer, D Peeters, E Tielens, AGGM Sauvage, M AF Martin-Hernandez, N. L. Schaerer, D. Peeters, E. Tielens, A. G. G. M. Sauvage, M. TI High spatial resolution mid-infrared spectroscopy of the starburst galaxies NGC3256, IIZw 40 and Henize 2-10 SO ASTRONOMY & ASTROPHYSICS LA English DT Review DE ISM : lines and bands; dust, extinction; HII regions; galaxies : starburst; infrared : galaxies ID H-II REGIONS; SPECTRAL ENERGY-DISTRIBUTIONS; COMPACT DWARF GALAXIES; MASSIVE STAR-FORMATION; WOLF-RAYET GALAXIES; POLYCYCLIC AROMATIC-HYDROCARBONS; INFRARED-EMISSION; MERGER NGC-3256; HII-REGIONS; MU-M AB Aims. In order to show the importance of high spatial resolution observations of extra-galactic sources when compared to observations obtained with larger apertures such as ISO, we present N-band spectra (8-13 mu m) of some locations in three starburst galaxies. In particular, we show the two galactic nuclei of the spiral galaxy NGC 3256, the compact IR supernebula in the dwarf galaxy II Zw40 and the two brightest IR knots in the central starburst of the WR galaxy He 2-10. Methods. The spectra were obtained with TIMMI2 on the ESO 3.6 m telescope. An inventory of the spectra in terms of atomic fine-structure lines and molecular bands is presented. Results. We show the value of these high spatial resolution data in constraining properties such as the extinction in the mid-IR, metallicity or stellar content (age, IMF, etc.). We have constrained the stellar content of the IR compact knot in II Zw40 by using the mid-IR fine-structure lines and setting restrictions on the nebular geometry. We have constructed a new mid-/far-IR diagnostic diagram based on the 11.2 mu m PAH and continuum, accessible to ground-based observations. We find that extra-galactic nuclei and star clusters observed at high spatial resolution ( as is the case of the TIMMI2 observations) are closer in PAH/far-IR to compact H-II regions, while galaxies observed by large apertures such as ISO are closer to exposed PDRs such as Orion. This is likely due to the aperture difference. We find a dependence between the presence of PAHs and the hardness of the radiation field as measured by the [S-IV]/[Ne-II] ratio that may be explained by the PAH-dust competition for FUV photons or the relative contribution of the different phases of the interstellar medium. C1 Inst Astrofis Canarias, Tenerife 38200, Spain. Observ Geneva, CH-1290 Sauverny, Switzerland. Observ Midi Pyrenees, UMR 5572, Lab Astrophys Toulouse Tarbes, F-31400 Toulouse, France. NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. SRON Netherlands Inst Space Res, NL-9700 AV Groningen, Netherlands. Kapteyn Inst, NL-9700 AV Groningen, Netherlands. CE Saclay, SAp, DAPNIA, CEA,DSM, F-91191 Gif Sur Yvette, France. RP Martin-Hernandez, NL (reprint author), Inst Astrofis Canarias, Via Lactea, Tenerife 38200, Spain. EM leticia@iac.es NR 121 TC 17 Z9 17 U1 0 U2 1 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD SEP PY 2006 VL 455 IS 3 BP 853 EP 870 DI 10.1051/0004-6361:20054302 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 074RN UT WOS:000239829600010 ER PT J AU Moehler, S Sweigart, AV AF Moehler, S. Sweigart, A. V. TI Observations of the hot horizontal-branch stars in the metal-rich bulge globular cluster NGC 6388 - Indications of helium enrichment and a lesson in crowded field spectroscopy SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE stars : horizontal; branch; stars : evolution; techniques : spectroscopic; Galaxy : bulge globular; clusters : individual : NGC 6388 ID DOUBLE MAIN-SEQUENCE; OMEGA-CENTAURI; NGC 6441; PHYSICAL PARAMETERS; MASS-DISTRIBUTION; VARIABLE-STARS; WHITE-DWARFS; HB STARS; CONSEQUENCES; ABUNDANCES AB Context. The metal-rich bulge globular cluster NGC 6388 shows a distinct blue horizontal-branch tail in its colour-magnitude diagram (Rich et al. 1997) and is thus a strong case of the well-known 2nd Parameter Problem. In addition, its horizontal branch (HB) shows an upward tilt toward bluer colours, which cannot be explained by canonical evolutionary models. Aims. Several noncanonical scenarios have been proposed to explain these puzzling observations. In order to test the predictions of these scenarios, we have obtained medium resolution spectra to determine the atmospheric parameters of a sample of the blue HB stars in NGC 6388. Methods. Using the medium resolution spectra, we determine effective temperatures, surface gravities and helium abundances by fitting the observed Balmer and helium lines with appropriate theoretical stellar spectra. As we know the distance to the cluster, we can verify our results by determining masses for the stars. During the data reduction we took special care in subtracting the background, which is dominated by the overlapping spectra of cool stars. Results. The cool blue tail stars in our sample with effective temperatures T(eff) approximate to 10 000 K have lower than canonical surface gravities, suggesting that these stars are, on average, similar to 0(m).4 brighter than canonical HB stars in agreement with the observed upward slope of the HB in NGC 6388. Moreover, the mean mass of these stars agrees well with theoretical predictions. In contrast, the hot blue tail stars in our sample with T(eff) >= 12 000 K show significantly lower surface gravities than predicted by any scenario, which can reproduce the photometric observations. Their masses are also too low by about a factor of 2 compared to theoretical predictions. Conclusions. The physical parameters of the blue HB stars near 10 000 K support the helium pollution scenario. The low gravities and masses of the hot blue tail stars, however, are probably caused by problems with the data reduction, most likely due to remaining background light in the spectra, which would affect the fainter hot blue tail stars much more strongly than the brighter cool blue tail stars. Our study of the hot blue tail stars in NGC 6388 illustrates the obstacles which are encountered when attempting to determine the atmospheric parameters of hot HB stars in very crowded fields using ground-based observations. We discuss these obstacles and offer possible solutions for future projects. C1 Inst Theoret Phys & Astrophys, D-24118 Kiel, Germany. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Moehler, S (reprint author), European So Observ, Karl Schwarzschild Str 2, D-85748 Garching, Germany. EM smoehler@eso.org OI Moehler, Sabine/0000-0002-4152-9643 NR 37 TC 25 Z9 25 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 SEP PY 2006 VL 455 IS 3 BP 943 EP 952 DI 10.1051/0004-6361:20065427 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 074RN UT WOS:000239829600018 ER PT J AU Levenson, NA Heckman, TM Krolik, JH Weaver, KA Zycki, P AF Levenson, N. A. Heckman, T. M. Krolik, J. H. Weaver, K. A. Zycki, P. T. TI Penetrating the deep cover of Compton-thick active galactic nuclei SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : active; galaxies : Seyfert; X-rays : galaxies ID NARROW-LINE REGION; X-RAY-EMISSION; LUMINOUS INFRARED GALAXIES; STAR-FORMING GALAXIES; SEYFERT 2 GALAXIES; XMM-NEWTON; CHANDRA OBSERVATIONS; PHYSICAL CONDITIONS; WARM ABSORBERS; ESO 428-G14 AB We analyze observations obtained with the Chandra X-Ray Observatory of bright Compton-thick active galactic nuclei (AGNs), those with column densities in excess of 1.5 x 10(24) cm(-2) along the lines of sight. We therefore view the powerful central engines only indirectly, even at X-ray energies. Using high spatial resolution and considering only galaxies that do not contain circumnuclear starbursts, we reveal the variety of emission AGNs alone may produce. Approximately 1% of the continuum's intrinsic flux is detected in reflection in each case. The only hard X-ray feature is the prominent Fe K alpha fluorescence line, with equivalent width greater than 1 keV in all sources. The Fe line luminosity provides the best X-ray indicator of the unseen intrinsic AGN luminosity. In detail, the morphologies of the extended soft X-ray emission and optical line emission are similar, and line emission dominates the soft X-ray spectra. Thus, we attribute the soft X-ray emission to material that the central engines photoionize. Because the resulting spectra are complex and do not reveal the AGNs directly, crude analysis techniques, such as hardness ratios, would misclassify these galaxies as hosts of intrinsically weak, unabsorbed AGNs and would fail to identify the luminous, absorbed nuclei that are present. We demonstrate that a three-band X-ray diagnostic can correctly classify Compton-thick AGNs, even when significant soft X-ray line emission is present. The active nuclei produce most of the galaxies' total observed emission over a broad spectral range, and much of their light emerges at far-infrared wavelengths. Stellar contamination of the infrared emission can be severe, however, making long-wavelength data alone unreliable indicators of the buried AGN luminosity. C1 Univ Kentucky, Dept Phys & Astron, Lexington, KY 40506 USA. Johns Hopkins Univ, Dept Phys & Astron, Bloomberg Ctr, Baltimore, MD 21218 USA. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Nicholas Copernicus Astron Ctr, PL-00716 Warsaw, Poland. RP Levenson, NA (reprint author), Univ Kentucky, Dept Phys & Astron, Lexington, KY 40506 USA. EM levenson@pa.uky.edu OI Levenson, Nancy A./0000-0003-4209-639X NR 81 TC 73 Z9 73 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 SEP 1 PY 2006 VL 648 IS 1 BP 111 EP 127 DI 10.1086/505735 PN 1 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 080EH UT WOS:000240230200011 ER PT J AU Kollmeier, JA Onken, CA Kochanek, CS Gould, A Weinberg, DH Dietrich, M Cool, R Dey, A Eisenstein, DJ Jannuzi, BT Le Floc'H, E Stern, D AF Kollmeier, Juna A. Onken, Christopher A. Kochanek, Christopher S. Gould, Andrew Weinberg, David H. Dietrich, Matthias Cool, Richard Dey, Arjun Eisenstein, Daniel J. Jannuzi, Buell T. Le Floc'H, Emeric Stern, Daniel TI Black hole masses and Eddington ratios at 0.3 < z < 4 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : active; galaxies : nuclei; surveys ID ACTIVE GALACTIC NUCLEI; BROAD-LINE REGION; FIBER-FED SPECTROGRAPH; DIGITAL SKY SURVEY; X-RAY SURVEY; HIGH-REDSHIFT; QUASARS; LUMINOSITY; GALAXIES; XBOOTES AB We study the distribution of Eddington luminosity ratios, L-bol/L-Edd, of active galactic nuclei (AGNs) discovered in the AGN and Galaxy Evolution Survey (AGES). We combine H beta, Mg II, and C IV line widths with continuum luminosities to estimate black hole (BH) masses in 407 AGNs, covering the redshift range z similar to 0.3-4 and the bolometric luminosity range L-bol similar to 10(45)-10(47) ergs s(-1). The sample consists of X-ray or mid-infrared (24 mu m) point sources with optical magnitude R <= 21.5 mag and optical emission-line spectra characteristic of AGNs. For the range of luminosity and redshift probed by AGES, the distribution of estimated Eddington ratios is well described as log-normal, with a peak at L-bol/L-Edd similar or equal to 1/4 and a dispersion of 0.3 dex. Since additional sources of scatter are minimal, this dispersion must account for contributions from the scatter between estimated and true BH mass and the scatter between estimated and true bolometric luminosity. Therefore, we conclude that (1) neither of these sources of error can contribute more than similar to 0.3 dex rms, and (2) the true Eddington ratios of optically luminous AGNs are even more sharply peaked. Because the mass estimation errors must be smaller than similar to 0.3 dex, we can also investigate the distribution of Eddington ratios at fixed BH mass. We show for the first time that the distribution of Eddington ratios at fixed BH mass is peaked, and that the dearth of AGNs at a factor of similar to 10 below Eddington is real and not an artifact of sample selection. These results provide strong evidence that supermassive BHs gain most of their mass while radiating close to the Eddington limit, and they suggest that the fueling rates in luminous AGNs are ultimately determined by BH self-regulation of the accretion flow rather than galactic-scale dynamical disturbances. C1 Ohio State Univ, Dept Astron, Columbus, OH 43210 USA. Herzberg Inst Astrophys, Victoria, BC V9E 2E7, Canada. Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. Natl Opt Astron Observ, Tucson, AZ 85719 USA. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Kollmeier, JA (reprint author), Ohio State Univ, Dept Astron, 140 W 18th Ave, Columbus, OH 43210 USA. EM jak@astronomy.ohio-state.edu; onken@astronomy.ohio-state.edu; ckochanek@astronomy.ohio-state.edu; gould@astronomy.ohio-state.edu; dhw@astronomy.ohio-state.edu; dietrich@astronomy.ohio-state.edu; rcool@as.arizona.edu; dey@noao.edu; isenste@cmb.as.arizona.edu; jannuzi@noao.edu OI Onken, Christopher/0000-0003-0017-349X NR 49 TC 274 Z9 274 U1 3 U2 11 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD SEP 1 PY 2006 VL 648 IS 1 BP 128 EP 139 DI 10.1086/505646 PN 1 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 080EH UT WOS:000240230200012 ER PT J AU Lieu, R Mittaz, JPD Zhang, SN AF Lieu, Richard Mittaz, Jonathan P. D. Zhang, Shuang-Nan TI The Sunyaev-Zel'dovich effect in a sample of 31 clusters: A comparison between the X-ray predicted and WMAP observed cosmic microwave background temperature decrement SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : clusters : general ID GALAXY CLUSTERS; DISTANCE SCALE; EMISSION; CONSTRAINTS; MAPS AB The WMAP Q-, V-, and W-band radial profiles of temperature deviation of the cosmic microwave background (CMB) were constructed for a sample of 31 randomly selected nearby clusters of galaxies in directions of Galactic latitude vertical bar b vertical bar > 30 degrees. The profiles were compared in detail with the expected CMB Sunyaev-Zel'dovich effect (SZE) caused by these clusters, with the hot gas properties of each cluster inferred observationally by applying gas temperatures as measured by ASCA to isothermal beta-models of the ROSAT X-ray surface brightness profiles, with the WMAP point-spread function fully taken into consideration. After co-adding the 31 cluster fields to significantly reduce the systematic and random uncertainties, it appears that WMAP detected the SZE in all three bands. Quantitatively, however, the observed SZE only accounts for about 1/4 of the expected decrement. The discrepancy represents too much unexplained extra flux: in the W band, the detected SZE corresponds on average to 5.6 times less X-ray gas mass within a 100 radius than the mass value given by the ROSAT beta-model. We critically examined how the X-ray prediction of the SZE may depend on our uncertainties in the density and temperature of the hot intracluster plasma, and emission by cluster radio sources. Although our comparison between the detected and expected SZE levels is subject to a margin of error, the fact remains that the average observed SZE depth and profile are consistent with those of the primary CMB anisotropy, i.e., the overall WMAP temperature decrement among the 31 rich clusters is too shallow to necessitate an interpretation in terms of an additional effect like the SZE. A unique aspect of this SZE investigation is that because all the data being analyzed are in the public domain, our work is readily open to scrutiny by others. C1 Univ Alabama, Dept Phys, Huntsville, AL 35899 USA. Tsing Hua Univ, Dept Phys, Beijing 100084, Peoples R China. Tsing Hua Univ, Ctr Astrophys, Beijing 100084, Peoples R China. Chinese Acad Sci, Key Lab Particle Astrophys, Inst High Energy Phys, Beijing 100039, Peoples R China. NASA, George C Marshall Space Flight Ctr, NSSTC, Huntsville, AL 35805 USA. RP Lieu, R (reprint author), Univ Alabama, Dept Phys, Huntsville, AL 35899 USA. NR 20 TC 37 Z9 37 U1 0 U2 3 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD SEP 1 PY 2006 VL 648 IS 1 BP 176 EP 199 DI 10.1086/505627 PN 1 PG 24 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 080EH UT WOS:000240230200017 ER PT J AU Loewenstein, M AF Loewenstein, Michael TI On iron enrichment, star formation, and type Ia supernovae in galaxy clusters SO ASTROPHYSICAL JOURNAL LA English DT Review DE galaxies : clusters : general; galaxies : evolution; stars : formation; supernovae : general; X-rays : galaxies : clusters ID INITIAL MASS FUNCTION; DIGITAL SKY SURVEY; MORPHOLOGY-DENSITY RELATION; NEAR-INFRARED PROPERTIES; K-BAND PROPERTIES; ULTRA-DEEP-FIELD; LY-ALPHA SURVEY; HIGH-REDSHIFT; INTRACLUSTER MEDIUM; ELLIPTIC GALAXIES AB The nature of star formation and SNe Ia in galaxies in the field and in rich galaxy clusters are contrasted by juxtaposing the buildup of heavy metals in the universe inferred from observed star formation and SN rate histories with data on the evolution of Fe abundances in the ICM. Models for the chemical evolution of Fe in these environments are constructed, subject to observational constraints, for this purpose. While models with a mean delay for SNe Ia of 3 Gyr and standard IMF are consistent with observations in the field, cluster Fe enrichment immediately tracks a rapid, top-heavy phase of star formation, although transport of Fe into the ICM may be more prolonged and star formation likely continues to redshifts < 1. The source of this prompt enrichment is SNe II yielding >= 0.1 M-circle dot per explosion ( if the SN Ia rate normalization is scaled down from its value in the field according to the relative number of candidate progenitor stars in the 3-8 M circle dot range) and/or SN Ia explosions with short delay times associated with the rapid star formation mode. Star formation is > 3 times more efficient in rich clusters than in the field, mitigating the over-cooling problem in numerical cluster simulations. Both the fraction of baryons cycled through stars and the fraction of the total present-day stellar mass in the form of stellar remnants are substantially greater in clusters than in the field. C1 NASA, Goddard Space Flight Ctr, High Energy Astrophys Lab, Greenbelt, MD 20771 USA. Univ Maryland, Dept Astron, College Pk, MD 20742 USA. RP Loewenstein, M (reprint author), NASA, Goddard Space Flight Ctr, High Energy Astrophys Lab, Code 662, Greenbelt, MD 20771 USA. EM loew@milkyway.gsfc.nasa.gov NR 126 TC 36 Z9 36 U1 0 U2 4 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD SEP 1 PY 2006 VL 648 IS 1 BP 230 EP 249 DI 10.1086/505648 PN 1 PG 20 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 080EH UT WOS:000240230200020 ER PT J AU Li, H Griffin, GS Krejny, M Novak, G Loewenstein, RF Newcomb, MG Calisse, PG Chuss, DT AF Li, H. Griffin, G. S. Krejny, M. Novak, G. Loewenstein, R. F. Newcomb, M. G. Calisse, P. G. Chuss, D. T. TI Results of SPARO 2003: Mapping magnetic fields in giant molecular clouds SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : magnetic fields; ISM : clouds; ISM : magnetic fields; polarization; turbulence ID H-II REGIONS; FAR-INFRARED POLARIMETRY; POLYCYCLIC AROMATIC-HYDROCARBONS; HIGH-RESOLUTION OBSERVATIONS; RECOMBINATION-LINE EMISSION; STAR-FORMATION; CARINA-NEBULA; MILKY-WAY; GRAIN ALIGNMENT; SUBMILLIMETER POLARIMETER AB We present results from the Austral Winter 2003 observing campaign of SPARO, a 450 mu m polarimeter used with a 2 m telescope at the South Pole. We mapped large-scale magnetic fields in four GMCs in the Galactic disk: NGC 6334, the Carina Nebula, G333.6-0.2, and G331.5-0.1. We find a statistically significant correlation of the inferred field directions with the orientation of the Galactic plane. Specifically, three of the four GMCs (NGC 6334 is the exception) have mean field directions that are within 15 degrees of the plane. The simplest interpretation is that the field direction tends to be preserved during the process of GMC formation. We have also carried out an analysis of published optical polarimetry data. For the closest of the SPARO GMCs, NGC 6334, we can compare the field direction in the cloud as measured by SPARO with the field direction in a larger region surrounding the cloud, as determined from optical polarimetry. For purposes of comparison, we also use optical polarimetry to determine field directions for 9-10 other regions of similar size. We find that the region surrounding NGC 6334 is an outlier in the distribution of field directions determined from optical polarimetry, just as the NGC 6334 cloud is an outlier in the distribution of cloud field directions determined by SPARO. In both cases the field direction corresponding to NGC 6334 is rotated away from the direction of the plane by a large angle. This finding is consistent with our suggestion that field direction tends to be preserved during GMC formation. Finally, by comparing the disorder in our magnetic field maps with the disorder seen in magnetic field maps derived from MHD turbulence simulations, we conclude that the magnetic energy density in our clouds is comparable to the turbulent energy density. C1 Northwestern Univ, Dept Phys & Astron, Evanston, IL 60208 USA. Yerkes Observ, Williams Bay, WI 53191 USA. Univ Cardiff Wales, Sch Phys & Astron, Cardiff CF24 3YB, Wales. NASA, Goddard Space Flight Ctr, High Energy Astrophys Lab, Greenbelt, MD 20771 USA. RP Li, H (reprint author), Northwestern Univ, Dept Phys & Astron, 2131 Sheridan Rd, Evanston, IL 60208 USA. EM h-li5@northwestern.edu RI Chuss, David/D-8281-2012 NR 89 TC 76 Z9 77 U1 0 U2 4 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD SEP 1 PY 2006 VL 648 IS 1 BP 340 EP 354 DI 10.1086/505858 PN 1 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 080EH UT WOS:000240230200027 ER PT J AU Smith, RK Dame, TM Costantini, E Predehl, P AF Smith, Randall K. Dame, T. M. Costantini, Elisa Predehl, Peter TI The X-ray halo of GX 5-1 SO ASTROPHYSICAL JOURNAL LA English DT Article DE dust, extinction; scattering; X-rays : binaries; X-rays : ISM ID INTERSTELLAR GRAINS; GALACTIC-CENTER; MILKY-WAY; INFRARED COUNTERPART; MOLECULAR CLOUDS; CO SURVEY; DUST; SCATTERING; EXTINCTION; BINARIES AB Using Chandra observations we have measured the energy-resolved dust-scattered X-ray halo around the low-mass X-ray binary GX 5-1, which shows signs of both singly and multiply scattered X-rays. We compared the observed X-ray halo at various energies to predictions from a range of dust models. These fits used both smoothly distributed dust and dust in clumped clouds, with CO and 21 cm observations helping to determine the positions of the clouds along the line of sight. We found that the BARE-GR-B model of Zubko and coworkers generally led to the best results, although inadequacies in both the overall model and the data limit our conclusions. We did find that the composite dust models of Zubko and coworkers, especially the "no carbon'' models, gave uniformly poor results. Although models using cloud positions and densities derived naively from CO and 21 cm data gave generally poor results, plausible adjustments to the distance of the largest cloud and the mass of a cloud in the expanding 3 kpc arm led to significantly improved fits. We suggest that combining X-ray halo, CO, and 21 cm observations will be a fruitful method to improve our understanding of both the gas and dust phases of the interstellar medium. C1 NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. SRON, Natl Inst Space Res, NL-3584 CA Utrecht, Netherlands. Univ Utrecht, Astron Inst, NL-3508 TA Utrecht, Netherlands. Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. RP Smith, RK (reprint author), NASA, Goddard Space Flight Ctr, Code 662, Greenbelt, MD 20771 USA. EM rsmith@milkyway.gsfc.nasa.gov NR 31 TC 17 Z9 17 U1 0 U2 3 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD SEP 1 PY 2006 VL 648 IS 1 BP 452 EP 460 DI 10.1086/505650 PN 1 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 080EH UT WOS:000240230200037 ER PT J AU Cushing, MC Roellig, TL Marley, MS Saumon, D Leggett, SK Kirkpatrick, JD Wilson, JC Sloan, GC Mainzer, AK Van Cleve, JE Houck, JR AF Cushing, Michael C. Roellig, Thomas L. Marley, Mark S. Saumon, D. Leggett, S. K. Kirkpatrick, J. Davy Wilson, John C. Sloan, G. C. Mainzer, Amy K. Van Cleve, Jeff E. Houck, James R. TI A Spitzer infrared spectrograph spectral sequence of M, L, and T dwarfs SO ASTROPHYSICAL JOURNAL LA English DT Article DE infrared : stars; stars : late-type; stars : low-mass, brown dwarfs ID ALL-SKY SURVEY; COOL BROWN DWARF; EPSILON-INDI-B; SPACE-TELESCOPE; ARRAY CAMERA; GLIESE 229B; ATMOSPHERIC CHEMISTRY; ENERGY-DISTRIBUTIONS; SPECTROSCOPIC SURVEY; SOLAR NEIGHBORHOOD AB We present a low-resolution (R lambda/Delta lambda approximate to 90), 5.5-38 mu m spectral sequence of a sample of M, L, and T dwarfs obtained with the Infrared Spectrograph ( IRS) on board the Spitzer Space Telescope. The spectra exhibit prominent absorption bands of H2O at 6.27 mu m, CH4 at 7.65 mu m, and NH3 at 10.5 mu m and are relatively featureless at lambda >= 15 mu m. Three spectral indices that measure the strengths of these bands are presented; H2O absorption features are present throughout the MLT sequence, while the CH4 and NH3 bands first appear at roughly the L/T transition. Although the spectra are, in general, qualitatively well matched by synthetic spectra that include the formation of spatially homogeneous silicate and iron condensate clouds, the spectra of the mid-type L dwarfs show an unexpected flattening from roughly 9 to 11 mu m. We hypothesize that this may be a result of a population of small silicate grains that are not predicted in the cloud models. The spectrum of the peculiar T6 dwarf 2MASS J0937 + 2931 is suppressed from 5.5 to 7.5 mu m relative to typical T6 dwarfs and may be a consequence of its mildly metal-poor/ high surface gravity atmosphere. Finally, we compute bolometric luminosities of a subsample of the M, L, and T dwarfs by combining the IRS spectra with previously published 0.6-4.1 mu m spectra and find good agreement with the values of Golimowski et al., who use L'-and M'-band photometry to account for the flux emitted at lambda > 2.5 mu m. C1 Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. NASA, Ames Res Ctr, Stanford, CA 94305 USA. Los Alamos Natl Lab, Div Appl Phys, Los Alamos, NM 87544 USA. Gemini No Operat, Hilo, HI 96720 USA. CALTECH, Infrared Proc & Anal Ctr, Pasadena, CA 91125 USA. Univ Virginia, Charlottesville, VA 22903 USA. Cornell Univ, Dept Astron, Ithaca, NY 14853 USA. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. Ball Aerosp & Technol Corp, Boulder, CO 80301 USA. Cornell Univ, Dept Astron, Ithaca, NY 14853 USA. RP Cushing, MC (reprint author), Univ Arizona, Steward Observ, 933 N Cherry Ave, Tucson, AZ 85721 USA. EM mcushing@as.arizona.edu; thomas.l.roellig@nasa.gov; mmarley@mail.arc.nasa.gov; dsaumon@lanl.gov; s.leggett@jach.hawaii.edu; davy@ipac.caltech.edu; jcw6z@virginia.edu; sloan@isc.astro.cornell.edu; amainzer@jpl.nasa.gov; jvanclev@ball.com OI Leggett, Sandy/0000-0002-3681-2989 NR 82 TC 95 Z9 95 U1 0 U2 4 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD SEP 1 PY 2006 VL 648 IS 1 BP 614 EP 628 DI 10.1086/505637 PN 1 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 080EH UT WOS:000240230200053 ER PT J AU Kastner, JH Richmond, M Grosso, N Weintraub, DA Simon, T Henden, A Hamaguchi, K Frank, A Ozawa, H AF Kastner, Joel H. Richmond, Michael Grosso, Nicolas Weintraub, David A. Simon, Theodore Henden, Arne Hamaguchi, Kenji Frank, Adam Ozawa, Hideki TI V1647 Orionis: The X-ray evolution of a pre-main-sequence accretion burst SO ASTROPHYSICAL JOURNAL LA English DT Article DE stars : formation; stars : individual (V1647 Orionis); stars : pre-main-sequence; X-rays : stars ID MCNEILS NEBULA; FU ORIONIS; YOUNG STAR; OUTBURST; IRAS-05436-0007; V1647-ORIONIS; VARIABILITY; EMISSION; SPECTRUM; CLUSTER AB We present Chandra X-Ray Observatory monitoring observations of the recent accretion outburst displayed by the pre-main-sequence (pre-MS) star V1647 Ori. The X-ray observations were obtained over a period beginning prior to outburst onset in late 2003 and continuing through its apparent cessation in late 2005, and demonstrate that the mean flux of the spatially coincident X-ray source closely tracked the near-infrared luminosity of V1647 Ori throughout its eruption. We find negligible likelihood that the correspondence between X-ray and infrared light curves over this period was the result of multiple X-ray flares unrelated to the accretion burst. The recent Chandra data confirm that the X-ray spectrum of V1647 Ori hardened during outburst, relative both to its preoutburst state and to the X-ray spectra of nearby pre-MS stars in the L1630 cloud. We conclude that the observed changes in the X-ray emission from V1647 Ori over the course of its 2003 - 2005 eruption were generated by a sudden increase and subsequent decline in its accretion rate. These results for V1647 Ori indicate that the flux of hard X-ray emission from erupting low-mass, pre-MS stars, and the duration and intensity of such eruptions, reflect the degree to which star-disk magnetic fields are reorganized before and during major accretion events. C1 Rochester Inst Technol, Rochester, NY 14623 USA. Univ Grenoble 1, Astrophys Lab Grenoble, F-38041 Grenoble, France. Vanderbilt Univ, Nashville, TN 37235 USA. Inst Astron, Honolulu, HI 96822 USA. USN Observ, Flagstaff Stn, Flagstaff, AZ 86002 USA. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Univ Space Res Assoc, Columbia, MD 21044 USA. Univ Rochester, Dept Phys & Astron, Rochester, NY 14627 USA. Osaka Univ, Grad Sch Sci, Dept Earth & Space Sci, Osaka 5600043, Japan. RP Kastner, JH (reprint author), Rochester Inst Technol, 54 Lomb Mem Dr, Rochester, NY 14623 USA. EM jhk@cis.rit.edu NR 32 TC 28 Z9 28 U1 0 U2 3 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD SEP 1 PY 2006 VL 648 IS 1 BP L43 EP L46 DI 10.1086/507992 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 080EI UT WOS:000240230300011 ER PT J AU Ueta, T Speck, AK Stencel, RE Herwig, F Gehrz, RD Szczerba, R Izumiura, H Zijlstra, AA Latter, WB Matsuura, M Meixner, M Steffen, M Elitzur, M AF Ueta, T. Speck, A. K. Stencel, R. E. Herwig, F. Gehrz, R. D. Szczerba, R. Izumiura, H. Zijlstra, A. A. Latter, W. B. Matsuura, M. Meixner, M. Steffen, M. Elitzur, M. TI Detection of a far-infrared bow shock nebula around R Hya: The first MIRIAD results SO ASTROPHYSICAL JOURNAL LA English DT Article DE circumstellar matter; infrared : stars; ISM : structure; stars : AGB and post-AGB; stars : individual (R Hydrae); stars : mass loss ID MULTIBAND IMAGING PHOTOMETER; SPITZER; EMISSION; SHELLS; HYDRAE; STARS; IRAS AB We present the first results of the MIRIAD (MIPS InfraRed Imaging of AGB Dust shells) project using the Spitzer Space Telescope. The primary aim of the project is to probe the material distribution in the extended circumstellar envelopes (CSEs) of evolved stars and recover the fossil record of their mass-loss history. Hence, we must map the whole of the CSEs plus the surrounding sky for background subtraction while avoiding the central star that is brighter than the detector saturation limit. With our unique mapping strategy, we have achieved better than 1 MJy sr(-1) sensitivity in 3 hr of integration and successfully detected a faint (< 5 MJy sr(-1)), extended (similar to 400") far-infrared nebula around the asymptotic giant branch (AGB) star R Hya. Based on the parabolic structure of the nebula, the direction of the space motion of the star with respect to the nebula shape, and the presence of extended Ha emission cospatial to the nebula, we suggest that the detected far-IR nebula is due to a bow shock at the interface of the interstellar medium and the AGB wind of this moving star. This is the first detection of the stellar-wind bow shock interaction for an AGB star and exemplifies the potential of Spitzer as a tool to examine the detailed structure of extended far-IR nebulae around bright central sources. C1 NASA, Ames Res Ctr, USRA, SOFIA Off, Moffett Field, CA 94035 USA. Univ Denver, Dept Phys & Astron, Denver, CO 80208 USA. Univ Missouri, Dept Phys & Astron, Columbia, MO 65211 USA. LANL, Theoret Astrophys Grp, Los Alamos, NM 87545 USA. Univ Minnesota, Dept Astron, Minneapolis, MN 55455 USA. Nicholas Copernicus Astron Ctr, PL-87100 Torun, Poland. Natl Astron Observ, Okayama Astrophys Observ, Asakuchi, Okayama 7190232, Japan. Univ Manchester, Sch Phys & Astron, Manchester M60 1QD, Lancs, England. CALTECH, NHSC, Pasadena, CA 91125 USA. Natl Astron Observ, Tokyo 1818588, Japan. STScI, Baltimore, MD 21218 USA. Astrophys Inst Potsdam, D-14482 Potsdam, Germany. Univ Kentucky, Dept Phys & Astron, Lexington, KY 40506 USA. RP Ueta, T (reprint author), NASA, Ames Res Ctr, USRA, SOFIA Off, MS 211-3, Moffett Field, CA 94035 USA. EM tueta@sofia.usra.edu NR 18 TC 53 Z9 53 U1 0 U2 3 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD SEP 1 PY 2006 VL 648 IS 1 BP L39 EP L42 DI 10.1086/507627 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 080EI UT WOS:000240230300010 ER PT J AU Kaneko, Y Preece, RD Briggs, MS Paciesas, WS Meegan, CA Band, DL AF Kaneko, Yuki Preece, Robert D. Briggs, Michael S. Paciesas, William S. Meegan, Charles A. Band, David L. TI The complete spectral catalog of bright batse gamma-ray bursts SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article ID SYNCHROTRON SHOCK MODEL; PROMPT EMISSION; EVOLUTION; PEAK; PULSES; SPECTROSCOPY; INTENSITY; BEHAVIOR AB We present a systematic spectral analysis of 350 bright gamma-ray bursts (GRBs) observed with the Burst and Transient Source Experiment (BATSE; similar to 30 keV-2 MeV) with high temporal and spectral resolution. Our sample was selected from the complete set of 2704 BATSE GRBs based on their energy fluence or peak photon flux values to assure good statistics and included 17 short GRBs. To obtain well-constrained spectral parameters, several photon models were used to fit each spectrum. We compared spectral parameters resulting from the fits using different models, and the spectral parameters that best represent each spectrum were statistically determined, taking into account the parameterization differences among the models. A thorough analysis was performed on 350 time-integrated and 8459 time-resolved burst spectra, and the effects of integration times in determining the spectral parameters were explored. Using the results, we studied correlations among spectral parameters and their evolution pattern within each burst. The resulting spectral catalog is the most comprehensive study of spectral properties of GRB prompt emission to date and is available electronically from the High-Energy Astrophysics Science Archive Research Center (HEASARC). The catalog provides reliable constraints on particle acceleration and emission mechanisms in GRBs. C1 Univ Space Res Assoc, NSSTC, Huntsville, AL 35805 USA. Univ Alabama, Dept Phys, NSSTC, Huntsville, AL 35805 USA. NASA, George C Marshall Space Flight Ctr, NSSTC, Huntsville, AL 35805 USA. Univ Maryland Baltimore Cty, Baltimore, MD 21250 USA. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Kaneko, Y (reprint author), Univ Space Res Assoc, NSSTC, VP-62,320 Sparkman Dr, Huntsville, AL 35805 USA. EM yuki.kaneko@nsstc.nasa.gov; rob.preece@nsstc.nasa.gov; michael.briggs@nsstc.nasa.gov; bill.paciesas@nsstc.nasa.gov; chip.meegan@nasa.gov; dband@milkyway.gsfc.nasa.gov OI Preece, Robert/0000-0003-1626-7335 NR 50 TC 277 Z9 281 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0067-0049 EI 1538-4365 J9 ASTROPHYS J SUPPL S JI Astrophys. J. Suppl. Ser. PD SEP PY 2006 VL 166 IS 1 BP 298 EP 340 DI 10.1086/505911 PG 43 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 082RD UT WOS:000240404000010 ER PT J AU Rutledge, CK Schuster, GL Charlock, TP Denn, FM Smith, WL Fabbri, BE Madigan, JJ Knapp, RJ AF Rutledge, Charles K. Schuster, Gregory L. Charlock, Thomas P. Denn, Frederick M. Smith, William L., Jr. Fabbri, Bryan E. Madigan, James J., Jr. Knapp, Robert J. TI Offshore radiation observations for climate research at the CERES ocean validation experiment - A new "laboratory" for retrieval algorithm testing SO BULLETIN OF THE AMERICAN METEOROLOGICAL SOCIETY LA English DT Article ID AEROSOL OPTICAL DEPTH; SKY RADIANCE MEASUREMENTS; CLAMS EXPERIMENT; CHESAPEAKE BAY; EAST-COAST; SURFACE; NETWORK; AERONET; WATER; CLOUDS C1 Analyt Serv & Mat Inc, Hampton, VA 23666 USA. NASA, Langley Res Ctr, Climate Sci Branch, Hampton, VA 23665 USA. Sci Applicat Int Corp, Hampton, VA 23665 USA. RP Rutledge, CK (reprint author), Suite 300,1 Enterprise Pkwy, Hampton, VA 23666 USA. EM c.k.rutledge@larc.nasa.gov NR 37 TC 6 Z9 6 U1 0 U2 0 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 0003-0007 J9 B AM METEOROL SOC JI Bull. Amer. Meteorol. Soc. PD SEP PY 2006 VL 87 IS 9 BP 1211 EP 1222 DI 10.1175/BAMS-87-9-1211 PG 12 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 089UY UT WOS:000240908000016 ER PT J AU Johanson, IA Fielding, EJ Rolandone, F Burgmann, R AF Johanson, Ingrid A. Fielding, Eric J. Rolandone, Frederique Burgmann, Roland TI Coseismic and postseismic slip of the 2004 Parkfield earthquake from space-geodetic data SO BULLETIN OF THE SEISMOLOGICAL SOCIETY OF AMERICA LA English DT Article ID SAN-ANDREAS-FAULT; GLOBAL POSITIONING SYSTEM; CALIFORNIA EARTHQUAKE; SURFACE DEFORMATION; HECTOR MINE; SUBSIDENCE; INTERFEROMETRY; CREEPMETERS; RECURRENCE; PREDICTION AB We invert interferometric synthetic aperture radar (InSAR) data jointly with campaign and continuous global positioning system (GPS) data for slip in the coseismic and postseismic periods of the 2004 Parkfield earthquake. The InSAR dataset consists of eight interferograms from data collected by the Envisat and Radarsat satellites spanning the time of the earthquake and variable amounts of the postseismic period. The two datasets complement each other, with the InSAR providing dense sampling of motion in the range direction of the satellite and the GPS providing more sparse, but three-dimensional measurements of ground motion. The model assumes exponential decay of the postseismic slip with a decay time constant of 0.087 years, determined from time series modeling of continuous GPS and creepmeter data. We find a geodetic moment magnitude of M 6.2 for a 1-day coseismic model and M-W 6.1 for the entire postseismic period. The coseismic rupture occurred mainly in two slip asperities; one near the hypocenter and the other 15-20 km north. Postseismic slip occurred on the shallow portions of the fault and near the rupture areas-of two M 5.0 aftershocks. A comparison of the geodetic slip models with seismic moment estimates suggests that the coseismic moment release of the Parkfield earthquake is as little as 25% of the total. This underlines the importance of aseismic slip in the slip budget for the Parkfield segment. C1 Univ Calif Berkeley, Berkeley Seismol Lab, Berkeley, CA 94027 USA. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. Univ Paris 06, Lab Tecton, CNRS, UMR 7072, F-75252 Paris 05, France. RP Johanson, IA (reprint author), US Geol Survey, 345 Middlefield Rd,MS 977, Menlo Pk, CA 94025 USA. EM ingrid@seismo.berkeley.edu RI Fielding, Eric/A-1288-2007 OI Fielding, Eric/0000-0002-6648-8067 NR 42 TC 79 Z9 79 U1 1 U2 12 PU SEISMOLOGICAL SOC AMER PI ALBANY PA 400 EVELYN AVE, SUITE 201, ALBANY, CA 94706-1375 USA SN 0037-1106 EI 1943-3573 J9 B SEISMOL SOC AM JI Bull. Seismol. Soc. Amer. PD SEP PY 2006 VL 96 IS 4 SU S BP S269 EP S282 DI 10.1785/0120050818 PN B PG 14 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 084MJ UT WOS:000240536800018 ER PT J AU Masson-Delmotte, V Kageyama, M Braconnot, P Charbit, S Krinner, G Ritz, C Guilyardi, E Jouzel, J Abe-Ouchi, A Crucifix, M Gladstone, RM Hewitt, CD Kitoh, A LeGrande, AN Marti, O Merkel, U Motoi, T Ohgaito, R Otto-Bliesner, B Peltier, WR Ross, I Valdes, PJ Vettoretti, G Weber, SL Wolk, F Yu, Y AF Masson-Delmotte, V. Kageyama, M. Braconnot, P. Charbit, S. Krinner, G. Ritz, C. Guilyardi, E. Jouzel, J. Abe-Ouchi, A. Crucifix, M. Gladstone, R. M. Hewitt, C. D. Kitoh, A. LeGrande, A. N. Marti, O. Merkel, U. Motoi, T. Ohgaito, R. Otto-Bliesner, B. Peltier, W. R. Ross, I. Valdes, P. J. Vettoretti, G. Weber, S. L. Wolk, F. Yu, Y. TI Past and future polar amplification of climate change: climate model intercomparisons and ice-core constraints (vol 26, pg 513, 2006) SO CLIMATE DYNAMICS LA English DT Correction C1 CEA Saclay, CNRS, UMR 1572, LSCE,IPSL, F-91191 Gif Sur Yvette, France. Ecole Natl Super Electrochim & Electrome Grenoble, Thermodynam & Physicochim Met Lab, CNRS, UMR 5183,UJF,Lab Glaciol & Geophys Environm, F-38402 St Martin Dheres, France. Univ Tokyo, Ctr Climate Syst Res, Kashiwa, Chiba 2778568, Japan. Hadley Ctr Climate Predict & Res, Exeter EX1 3PB, Devon, England. Univ Bristol, Sch Geog Sci, Bristol BS8 1SS, Avon, England. Meteorol Res Inst, Climate Res Dept, Tsukuba, Ibaraki 3050052, Japan. Columbia Univ, NASA, Goddard Inst Space Studies, New York, NY USA. Columbia Univ, NASA, Ctr Climate Syst Res, New York, NY USA. GEOMAR, IFM, D-24105 Kiel, Germany. JAMSTEC, FRCGC, Yokohama, Kanagawa 2360001, Japan. Natl Ctr Atmospher Res, Climate Change Res, Boulder, CO 80307 USA. Univ Toronto, Dept Phys, Toronto, ON M5S 1A7, Canada. Royal Netherlands Meteorol Inst, NL-3730 AE De Bilt, Netherlands. Univ Catholique Louvain, Inst Astron & Geofis G Lemaitre, B-1348 Louvain, Belgium. Chinese Acad Sci, Inst Atmospher Phys, LASG, New York, NY 10029 USA. RP Masson-Delmotte, V (reprint author), CEA Saclay, CNRS, UMR 1572, LSCE,IPSL, Batimento 701, F-91191 Gif Sur Yvette, France. EM valerie.masson@cea.fr RI Marti, Olivier/B-2378-2009; KAGEYAMA, Masa/F-2389-2010; Yu, Yongqiang /K-7808-2012; Ross, Ian/C-8766-2011; Krinner, Gerhard/A-6450-2011; LeGrande, Allegra/D-8920-2012; Peltier, William/A-1102-2008; Masson-Delmotte, Valerie/G-1995-2011; Gladstone, Rupert/C-1086-2013; Valdes, Paul/C-4129-2013; Abe-Ouchi, Ayako/M-6359-2013 OI KAGEYAMA, Masa/0000-0003-0822-5880; Yu, Yongqiang /0000-0001-8596-3583; Krinner, Gerhard/0000-0002-2959-5920; LeGrande, Allegra/0000-0002-5295-0062; Masson-Delmotte, Valerie/0000-0001-8296-381X; Gladstone, Rupert/0000-0002-1582-3857; Abe-Ouchi, Ayako/0000-0003-1745-5952 NR 1 TC 9 Z9 10 U1 1 U2 11 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0930-7575 J9 CLIM DYNAM JI Clim. Dyn. PD SEP PY 2006 VL 27 IS 4 BP 437 EP 440 DI 10.1007/s00382-006-0149-1 PG 4 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 061BY UT WOS:000238847400008 ER PT J AU Brown, ME Pinzon, JE Prince, SD AF Brown, Molly E. Pinzon, Jorge E. Prince, Stephen D. TI The effect of vegetation productivity on millet prices in the informal markets of Mali, Burkina Faso and Niger SO CLIMATIC CHANGE LA English DT Article; Proceedings Paper CT Conference on Adaptive Research and Governance in Climate Change CY OCT, 2003 CL Ohio State Univ, Columbus, OH SP Climate Change & Environm Res Initiat, Environm Policy Initiat, Mershon Ctr, Cluster Interdisciplinary Res Int Themes HO Ohio State Univ ID NDVI DATA; COPING STRATEGIES; SAHEL; MODEL; BEHAVIOR; AFRICA AB Systematic evaluation of food security throughout the Sahel has been attempted for nearly two decades. Food security analyses have used both food prices to determine the ability of the population to access food, and satellite-derived vegetation indices that measure vegetation production to establish how much food is available each year. The relationship between these two food security indicators is explored here using correspondence analysis and through the use of Markov chain models. Two sources of quantitative data were used: 8 km normalized difference vegetation index (NDVI) data from the Advanced Very High Resolution Radiometers (AVHRR) carried on the NOAA series of satellites, and monthly millet prices from 445 markets in Mali, Niger and Burkina Faso. The results show that the growing season vegetation production is related to the price of millet at the annual and the seasonal time scales. If the growing season was characterized by erratic, sparse rainfall, it resulted in higher prices, and well-distributed, abundant rainfall resulted in lower prices. The correspondence between vegetation production and millet prices is used to produce maps of millet prices for West Africa. C1 Univ Maryland, NASA, Goddard Space Flight Ctr, Dept Geog, Greenbelt, MD 20771 USA. NASA, Goddard Space Flight Ctr, Sci Syst & Applicat Inc, Greenbelt, MD 20771 USA. Univ Maryland, Dept Geog, College Pk, MD 20742 USA. RP Brown, ME (reprint author), Univ Maryland, NASA, Goddard Space Flight Ctr, Dept Geog, Code 923, Greenbelt, MD 20771 USA. EM molly.brown@gsfc.nasa.gov RI Brown, Molly/E-2724-2010; Brown, Molly/M-5146-2013 OI Brown, Molly/0000-0001-7384-3314; Brown, Molly/0000-0001-7384-3314 NR 51 TC 11 Z9 11 U1 0 U2 3 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0165-0009 J9 CLIMATIC CHANGE JI Clim. Change PD SEP PY 2006 VL 78 IS 1 BP 181 EP 202 DI 10.1007/s10584-006-9096-4 PG 22 WC Environmental Sciences; Meteorology & Atmospheric Sciences SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences GA 083UY UT WOS:000240484900008 ER PT J AU Tezduyar, TE Senga, M Vicker, D AF Tezduyar, TE Senga, M Vicker, D TI Computation of inviscid supersonic flows around cylinders and spheres with the SUPG formulation and Y Z beta shock-capturing SO COMPUTATIONAL MECHANICS LA English DT Article; Proceedings Paper CT 13th Conference on Finite Elements for Flow Problems CY APR 04-06, 2005 CL Swansea, WALES DE supersonic flows; cylinders and spheres; SUPG stabilization; stabilization parameter; shock-capturing parameter ID FINITE-ELEMENT FORMULATION; ADVECTIVE-DIFFUSIVE SYSTEMS; NAVIER-STOKES EQUATIONS; SPACE-TIME PROCEDURE; FLUID-DYNAMICS; MOVING BOUNDARIES; COMPRESSIBLE EULER; INTERFACES; EMPHASIS; STRATEGY AB Numerical experiments with inviscid supersonic flows around cylinders and spheres are carried out to evaluate the stabilization and shock-capturing parameters introduced recently for the Streamline-Upwind/Petrov-Galerkin (SUPG) formulation of compressible flows based on conservation variables. The tests with the cylinders are carried out for both structured and unstructured meshes. The new shock-capturing parameters, which we call "YZ beta Shock-Capturing", are compared to earlier SUPG parameters derived based on the entropy variables. In addition to being much simpler, the new shock-capturing parameters yield better shock quality in the test computations, with more substantial improvements seen for unstructured meshes with triangular and tetrahedral elements. Furthermore, the results obtained with YZ beta Shock-Capturing compare very favorably to those obtained with the well established OVERFLOW code. C1 Rice Univ, Dept Mech Engn, Houston, TX 77005 USA. NASA, Appl Aerosci & CFD Branch, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. RP Tezduyar, TE (reprint author), Rice Univ, Dept Mech Engn, MS 321,6100 Main St, Houston, TX 77005 USA. EM tezduyar@rice.edu; msenga@rice.edu; darby.vicker-1@nasa.gov RI Tezduyar, Tayfun/F-6134-2012 OI Tezduyar, Tayfun/0000-0001-8707-3162 NR 23 TC 46 Z9 46 U1 0 U2 6 PU SPRINGER PI NEW YORK PA 233 SPRING STREET, NEW YORK, NY 10013 USA SN 0178-7675 J9 COMPUT MECH JI Comput. Mech. PD SEP PY 2006 VL 38 IS 4-5 BP 469 EP 481 DI 10.1007/s00466-005-0025-6 PG 13 WC Mathematics, Interdisciplinary Applications; Mechanics SC Mathematics; Mechanics GA 057YW UT WOS:000238632100016 ER PT J AU Przekop, A Rizzi, SA AF Przekop, Adam Rizzi, Stephen A. TI A reduced order method for predicting high cycle fatigue of nonlinear structures SO COMPUTERS & STRUCTURES LA English DT Article; Proceedings Paper CT 7th International Conference on Computational Structures Technology/4th International Conference on Engineering Computational Technology CY SEP 07-09, 2004 CL Lisbon, PORTUGAL DE nonlinear random response; high-cycle-fatigue; reduced order methods AB The goal of this investigation is to assess the quality of high-cycle-fatigue life estimation via a reduced order method for structures undergoing geometrically nonlinear random vibrations. Modal reduction is performed with several different suites of basis functions. After numerically solving the reduced order system equations of motion, the physical displacement time history is obtained by an inverse transformation and stresses are recovered. Stress ranges obtained through the rainflow counting procedure are used in a linear damage accumulation method to yield fatigue estimates. Fatigue life estimates obtained using various basis functions in the reduced order method are compared with those obtained from numerical simulation in physical degrees-of-freedom. (c) 2006 Civil-Comp Ltd. and Elsevier Ltd. All rights reserved. C1 NASA, Langley Res Ctr, Natl Inst Aerosp, Struct Acoust Branch, Hampton, VA 23681 USA. Natl Inst Aerosp, Hampton, VA 23666 USA. RP Przekop, A (reprint author), NASA, Langley Res Ctr, Natl Inst Aerosp, Struct Acoust Branch, MC 463, Hampton, VA 23681 USA. EM adam@nianet.org NR 21 TC 9 Z9 9 U1 0 U2 2 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0045-7949 J9 COMPUT STRUCT JI Comput. Struct. PD SEP PY 2006 VL 84 IS 24-25 BP 1606 EP 1618 DI 10.1016/j.compstruc.2006.01.015 PG 13 WC Computer Science, Interdisciplinary Applications; Engineering, Civil SC Computer Science; Engineering GA 082MH UT WOS:000240390400006 ER PT J AU Sullivan, MC Cowen, RK Able, KW Fahay, MP AF Sullivan, Mark C. Cowen, Robert K. Able, Kenneth W. Fahay, Michael P. TI Applying the basin model: Assessing habitat suitability of young-of-the-year demersal fishes on the New York Bight continental shelf SO CONTINENTAL SHELF RESEARCH LA English DT Article DE habitat; recruitment; young-of-the-year; submersible; continental shelf; USA; Northwest Atlantic; New York Bight ID FLOUNDER LIMANDA-FERRUGINEA; MIDDLE ATLANTIC BIGHT; NURSERY HABITAT; SETTLEMENT; GROWTH; RECRUITMENT; FLATFISH; SIZE; POPULATION; MORTALITY AB The extent to which young-of-the-year (YOY) fish habitats become saturated with new recruits has remained relatively unevaluated for temperate, demersal, continental shelf fishes. MacCall's [1990. Dynamic Geography of Marine Fish Populations. Washington Sea Grant Program, University of Washington Press, Seattle, Washington] basin model was used as a framework for examining the dynamics of an assemblage of recently settled fishes in relation to available microhabitat on the New York Bight continental shelf (USA). For four abundant species (three flatfish, one merlucciid hake), density-specific patterns of microhabitat selection, spatial dispersion and overall cross-shelf habitat use were investigated using a research submersible over three cross-shelf transects during the late summer settlement season. Typically, recruits that saturated YOY habitats (> 1 ind/m(2)) were randomly distributed within underwater transects and formed weak associations with specific microhabitats. At lower densities (< 1 ind/m2), recruit spacing tended toward nonrandom (clumped/even) with increasing significant affinities for ecologically important substrates (i.e. Limanda ferruginea, sand wave crests/low shell hash). For Citharichthys arctifrons, clumping appeared to increase with complexity of the habitat. Several less-abundant species (i.e. Urophycis chuss, Tautogolabrus adspersus) formed tight associations with rare habitat features and may consequently encounter the greatest bottleneck for space during the benthic/pelagic transition. Although restricted by the scale of observation, these results begin to elucidate the mechanisms by which habitat quality and quantity moderate recruitment on the continental shelf. (c) 2006 Elsevier Ltd. All rights reserved. C1 Univ Miami, Rosenstiel Sch Marine & Atmospher Sci, Div Marine Biol & Fisheries, Miami, FL 33149 USA. Rutgers State Univ, Marine Field Stn, Inst Marine & Coastal Sci, Tickerton, NJ USA. James J Howard Marine Sci Lab, Natl Marine Fisheries Serv, NE Fisheries Sci Ctr, Highlands 07732, NJ USA. RP Sullivan, MC (reprint author), Stockton State Coll, Marine Sci Program, Div Nat Sci & Math, POB 195, Pomona, NJ 08240 USA. EM Mark.Sullivan@stockton.edu NR 33 TC 7 Z9 7 U1 0 U2 3 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0278-4343 J9 CONT SHELF RES JI Cont. Shelf Res. PD SEP PY 2006 VL 26 IS 14 BP 1551 EP 1570 DI 10.1016/j.csr.2006.03.012 PG 20 WC Oceanography SC Oceanography GA 088CQ UT WOS:000240789500002 ER PT J AU Gruber, N Frenzel, H Doney, SC Marchesiello, P McWilliams, JC Moisan, JR Oram, JJ Plattner, GK Stolzenbach, KD AF Gruber, Nicolas Frenzel, Hartmut Doney, Scott C. Marchesiello, Patrick McWilliams, James C. Moisan, John R. Oram, John J. Plattner, Gian-Kasper Stolzenbach, Keith D. TI Eddy-resolving simulation of plankton ecosystem dynamics in the California Current System SO DEEP-SEA RESEARCH PART I-OCEANOGRAPHIC RESEARCH PAPERS LA English DT Article DE phytoplankton dynamics; nutrient cycling; coastal biogeochemistry; California current; upwelling ID GENERAL-CIRCULATION MODEL; GLOBAL CARBON-CYCLE; NORTH-ATLANTIC; PHYTOPLANKTON GROWTH; CONTINENTAL MARGINS; UPWELLING SYSTEM; TRANSITION ZONE; ORGANIC-CARBON; CRITICAL DEPTH; COASTAL ZONE AB We study the dynamics of the planktonic ecosystem in the coastal upwelling zone within the California Current System using a three-dimensional (3-D), eddy-resolving circulation model coupled to an ecosystern/biogeochemistry model. The physical model is based on the Regional Oceanic Modeling System (ROMS), configured at a resolution of 15 km for a domain covering the entire US West Coast, with an embedded child grid covering the central California upwelling region at a resolution of 5 km. The model is forced with monthly mean boundary conditions at the open lateral boundaries as well as at the surface. The ecological/biogeochemical model is nitrogen based, includes single classes for phytoplankton and zooplankton, and considers two detrital pools with different sinking speeds. The model also explicitly simulates a variable chlorophyll-to-carbon ratio. Comparisons of model results with either remote sensing observations (AVHRR, SeaWiFS) or in-situ measurements from the CalCOFI program indicate that our model is capable of replicating many of the large-scale, time-averaged features of the coastal upwelling system. An exception is the underestimation of the chlorophyll levels in the northern part of the domain, perhaps because of the lack of short-term variations in the atmospheric forcing. Another shortcoming is that the modeled thermocline is too diffuse, and that the upward slope of the isolines toward the coast is too small. Detailed time-series comparisons with observations from Monterey Bay reveal similar agreements and discrepancies. We attribute the good agreement between the modeled and observed ecological properties in large part to the accuracy of the physical fields. In turn, many of the discrepancies can be traced back to our use of monthly mean forcing. Analysis of the ecosystem structure and dynamics reveal that the magnitude and pattern of phytoplankton biomass in the nearshore region are determined largely by the balance of growth and zooplankton grazing, while in the offshore region, growth is balanced by mortality. The latter appears to be inconsistent with in situ observations and is a result of our consideration of only one zooplankton size class (mesozooplankton), neglecting the importance of microzooplankton grazing in the offshore region. A comparison of the allocation of nitrogen into the different pools of the ecosystem in the 3-D results with those obtained from a box model configuration of the same ecosystem model reveals that only a few components of the ecosystem reach a local steady-state, i.e. where biological sources and sinks balance each other. The balances for the majority of the components are achieved by local biological source and sink terms balancing the net physical divergence, confirming the importance of the 3-D nature of circulation and mixing in a coastal upwelling system. (c) 2006 Elsevier Ltd. All rights reserved. C1 Univ Calif Los Angeles, Inst Geophys & Planet Phys, Los Angeles, CA 90095 USA. Univ Calif Los Angeles, Dept Atmospher & Ocean Sci, Los Angeles, CA 90095 USA. Univ Calif Los Angeles, CH-8006 Zurich, Switzerland. NASA, Goddard Space Flight Ctr, Wallops Flight Facil, Observat Sci Branch,Lab Hydrospher Proc, Wallops Isl, VA 23337 USA. Woods Hole Oceanog Inst, Dept Marine Chem & Geochem, Woods Hole, MA 02543 USA. IRD Ctr Bretagne, Plouzane, France. RP Gruber, N (reprint author), ETH, Inst Biogeochem & Pollut Dynam, CH-8006 Zurich, Switzerland. EM nicolas.gruber@env.ethz.ch RI Gruber, Nicolas/B-7013-2009; Doney, Scott/F-9247-2010; Moisan, John/B-8762-2016; Plattner, Gian-Kasper/A-5245-2016 OI Gruber, Nicolas/0000-0002-2085-2310; Doney, Scott/0000-0002-3683-2437; Moisan, John/0000-0002-8078-8939; Plattner, Gian-Kasper/0000-0002-3765-0045 NR 82 TC 97 Z9 99 U1 2 U2 38 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0967-0637 EI 1879-0119 J9 DEEP-SEA RES PT I JI Deep-Sea Res. Part I-Oceanogr. Res. Pap. PD SEP PY 2006 VL 53 IS 9 BP 1483 EP 1516 DI 10.1016/j.dsr.2006.06.005 PG 34 WC Oceanography SC Oceanography GA 106UF UT WOS:000242126500003 ER PT J AU Jackson, J Bouchon, M Fielding, E Funning, G Ghorashi, M Hatzfeld, D Nazari, H Parsons, B Priestley, K Talebian, M Tatar, M Walker, R Wright, T AF Jackson, J. Bouchon, M. Fielding, E. Funning, G. Ghorashi, M. Hatzfeld, D. Nazari, H. Parsons, B. Priestley, K. Talebian, M. Tatar, M. Walker, R. Wright, T. TI Seismotectonic, rupture process, and earthquake-hazard aspects of the 2003 December 26 Bam, Iran, earthquake SO GEOPHYSICAL JOURNAL INTERNATIONAL LA English DT Article DE active faulting; continental tectonics; earthquakes; InSAR; Iran; seismology ID ACTIVE TECTONICS; SOURCE PARAMETERS; SOUTHEAST IRAN; SE IRAN; FAULT SYSTEM; COSEISMIC DEFORMATION; RADAR INTERFEROMETRY; SURFACE DEFORMATION; EASTERN IRAN; THRUST BELT AB The catastrophic 2003 M-w 6.6 Bam earthquake in southern Iran attracted much attention, and has been studied with an abundance of observations from synthetic aperture radar, teleseismic seismology, aftershock studies, strong ground motion, geomorphology, remote sensing and surface field work. Many reports have focused on the details of one or other data type, producing interpretations that either conflict with other data or leave questions unanswered. This paper is an attempt to look at all the available data types together, to produce a coherent picture of the coseismic faulting in 2003 and to examine its consequences for active tectonics and continuing seismic hazard in the region. We conclude that more than 80 per cent of the moment release in the main shock occurred on a near-vertical right-lateral strike-slip fault extending from the city of Bam southwards for about 15 km, with slip of up to 2 m but mostly restricted to the depth range 2-7 km. Analysis of the strong ground motion record at Bam is consistent with this view, and indicates that the extreme damage in the city can be attributed, at least in part, to the enhancement of ground motion in Bam because of its position at the end of the northward-propagating rupture. Little of the slip in the main shock reached the Earth's surface and, more importantly, aftershocks reveal that similar to 12 km vertical extent of a deeper part of the fault system remained unruptured beneath the coseismic rupture plane, at depths of 8-20 km. This may represent a substantial remaining seismic hazard to the reconstructed city of Bam. We believe that some oblique-reverse slip (up to 2 m, and less than 20 per cent of the released seismic moment) occurred at a restricted depth of 5-7 km on a blind west-dipping fault that projects to the surface at the Bam-Baravat escarpment, an asymmetric anticline ridge that is the most prominent geomorphological feature in the area. This fault did not rupture significantly at shallow levels in 2003, and it may also represent a continuing seismic hazard. Widespread distributed surface ruptures north of the city are apparently unrelated to substantial slip at depth, and may be the result of enhanced ground motion related to northward propagation of the rupture. The faulting at Bam may be in the early stages of a spatial separation ('partitioning') between the reverse and strike-slip components of an oblique convergence across the zone. Such a separation is common on the continents, though in this case the slip vectors between the two faults differ only by similar to 20 degrees as a substantial strike-slip component remains on the oblique-reverse fault. The Bam earthquake is one in a series of large earthquakes involving faulting along the western edge of the Lut desert. In addition to the unruptured parts of the faults near Bam itself, continuing and substantial hazard is represented by unruptured neighbouring faults, particularly blind thrusts along the Jebel Barez mountains to the south and strike-slip faulting at Sarvestan to the west. C1 COMET, Bullard Labs, Cambridge CB3 0EZ, England. CNRS, UJF, Lab Geophys Interne & Tectonophys, Grenoble, France. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. COMET, Dept Earth Sci, Oxford OX1 3PR, England. Geol Survey Iran, Tehran, Iran. Int Inst Earthquake Engn & Seismol, Tehran, Iran. RP Jackson, J (reprint author), COMET, Bullard Labs, Madingley Rd, Cambridge CB3 0EZ, England. EM jackson@esc.cam.ac.uk RI Walker, Richard/D-9908-2011; Funning, Gareth/F-6926-2011; Wright, Tim/A-5892-2011; Parsons, Barry/K-4716-2012; NCEO, COMET+`/A-3443-2013; Fielding, Eric/A-1288-2007; OI Wright, Tim/0000-0001-8338-5935; Fielding, Eric/0000-0002-6648-8067; Funning, Gareth/0000-0002-8247-0545 NR 63 TC 59 Z9 60 U1 1 U2 6 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0956-540X EI 1365-246X J9 GEOPHYS J INT JI Geophys. J. Int. PD SEP PY 2006 VL 166 IS 3 BP 1270 EP 1292 DI 10.1111/j.1365-246X.2006.03056.x PG 23 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 075DF UT WOS:000239862300019 ER PT J AU Shilling, JE Tolbert, MA Toon, OB Jensen, EJ Murray, BJ Bertram, AK AF Shilling, J. E. Tolbert, M. A. Toon, O. B. Jensen, E. J. Murray, B. J. Bertram, A. K. TI Measurements of the vapor pressure of cubic ice and their implications for atmospheric ice clouds SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID X-RAY-DIFFRACTION; AMORPHOUS WATER ICE; LOW-TEMPERATURE; HEXAGONAL ICE; CIRRUS CLOUDS; ASTROPHYSICAL IMPLICATIONS; ELECTRON DIFFRACTION; GLASSY WATER; SPECTRA; FORMS AB Under conditions commonly found in Earth's atmosphere, water can form two solid phases; hexagonal ice (I-h) and cubic ice (I-c). Recent reports have suggested that Ic may form in the atmosphere under a wider range of conditions than previously believed. In light of these reports, the formation of Ic has been suggested as one contributing factor for in-situ observations of persistent in-cloud supersaturations in cold cirrus. However, an accurate evaluation of the contribution of Ic formation to the observed supersaturations requires knowledge of the saturation vapor pressure of Ic, which has not been measured. In this manuscript, we report direct measurements of the vapor pressure of Ic over the temperature range 180 - 190 K. Over this temperature range, the vapor pressure of the cubic phase is 10.5 +/- 2.5% higher than that of the hexagonal phase. Field measurements of in-cloud supersaturations made during CRYSTAL-FACE are also re-analyzed and discussed. C1 Univ Colorado, Dept Chem & Biochem, Boulder, CO 80309 USA. Univ Colorado, Cooperat Inst Res Environm Sci, Boulder, CO 80309 USA. Univ Colorado, Atmospher & Space Phys Lab, Program Atmospher & Ocean Sci, Boulder, CO 80309 USA. NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. Univ British Columbia, Dept Chem, Vancouver, BC V6T 1Z1, Canada. RP Shilling, JE (reprint author), Harvard Univ, Div Engn & Appl Sci, 40 Oxford St, Cambridge, MA 02138 USA. EM shilling@deas.harvard.edu; tolbert@colorado.edu; toon@lasp.colorado.edu; ejensen@cirrus.arc.nasa.gov; bmurray@chem.ubc.ca; bertram@chem.ubc.ca RI Murray, Benjamin/C-1219-2010; Shilling, John/L-6998-2015 OI Murray, Benjamin/0000-0002-8198-8131; Shilling, John/0000-0002-3728-0195 NR 38 TC 53 Z9 53 U1 3 U2 20 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 EI 1944-8007 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD SEP 1 PY 2006 VL 33 IS 17 AR L17801 DI 10.1029/2006GL026671 PG 5 WC Geosciences, Multidisciplinary SC Geology GA 081QH UT WOS:000240331600005 ER PT J AU Gerhard, L AF Gerhard, Lee TI Testing global warming hypotheses SO GEOTIMES LA English DT Editorial Material C1 NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Gerhard, L (reprint author), NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. NR 0 TC 0 Z9 0 U1 0 U2 1 PU AMER GEOLOGICAL INST PI ALEXANDRIA PA 4220 KING ST, ALEXANDRIA, VA 22302-1507 USA SN 0016-8556 J9 GEOTIMES JI Geotimes PD SEP PY 2006 VL 51 IS 9 BP 7 EP + PG 2 WC Geosciences, Multidisciplinary SC Geology GA 081MN UT WOS:000240321800006 ER PT J AU Ramillien, G Lombard, A Cazenave, A Ivins, ER Llubes, M Remy, F Biancale, R AF Ramillien, G. Lombard, A. Cazenave, A. Ivins, E. R. Llubes, M. Remy, F. Biancale, R. TI Interannual variations of the mass balance of the Antarctica and Greenland ice sheets from GRACE SO GLOBAL AND PLANETARY CHANGE LA English DT Article DE ice sheets mass balance; GRACE satellite gravimetry; sea level ID SEA-LEVEL RISE; TIME VARIATIONS; GRAVITY-FIELD; WATER STORAGE; VARIABILITY; TEMPERATURE; INVERSION; GROWTH; EARTH; MODEL AB We propose a new estimate of the mass balance of the West/East Antarctica and Greenland ice sheets from GRACE for the recent period (July 2002-March 2005) and compute the corresponding contribution to the global mean sea level. We use new GRACE geoid solutions provided by the Groupe de Recherche en Geodesie Spatiale (GRGS/CNES), at the resolution of similar to 400 km and sampled at 10-day interval. In the three regions, significant interannual variations are observed, which we approximate as linear trends over the short time span of analysis. Over Greenland, an apparent total volume loss of 119 +/-10 cu km/yr water is observed. For the Antarctica ice sheet, a bimodal behaviour is apparent, with volume loss amounting to 88 +/- 10 cu km/yr water in the West, and increase in the East amounting to 72 +/-20 cu km/yr water. These GRACE results are affected by land hydrology contamination and glacial isostatic adjustment (GIA) of the solid Earth since last deglaciation. We correct for both land hydrology contamination (using a global hydrological model) and GIA using the ICE-4G model for Greenland and the IJ05 model for Antarctica. Corrected for both land hydrology contamination and GIA, GRACE volume rates are - 129 +/-15 cu km/yr, - 107 +/ -23 cu km/yr and +67 +/-28 cu km/yr for Greenland, West Antarctica and East Antarctica respectively. In terms of sea level rise, the GRACE-based ice sheets contributions are +0.36 +/-0.04 mm/yr for Greenland, +0.30 +/- 0.06 mm/yr for West Antarctica and - 0.19 +/- 0.07 for East Antarctica for the time interval of study. The total Antarctica contribution to sea level over this short time span is thus slightly positive (+0.11 +/-0.09 mm/yr). The ice sheets together contribute to a sea level rise of 0.47 +/-0.1 mm/yr. The results reported here are in qualitative agreement with recent estimates of the mass balance of the ice sheets based on GRACE and with those based upon other remote sensing observations. Due to the very short sampling time span for which the GRACE data are available, it is not yet possible to distinguish between interannual oscillations and long-term trend associated with climate change. (C) 2006 Elsevier B.V. All rights reserved. C1 Observ Midi Pyrenees, LEGOS, F-31401 Toulouse 9, France. CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. CNES, Grp Geodesie Spatiale, Toulouse, France. RP Ramillien, G (reprint author), Observ Midi Pyrenees, LEGOS, 18 Ave E Belin, F-31401 Toulouse 9, France. EM ramillie@notos.cst.cnes.fr NR 41 TC 135 Z9 145 U1 4 U2 35 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0921-8181 EI 1872-6364 J9 GLOBAL PLANET CHANGE JI Glob. Planet. Change PD SEP PY 2006 VL 53 IS 3 BP 198 EP 208 DI 10.1016/j.gloplacha.2006.06.003 PG 11 WC Geography, Physical; Geosciences, Multidisciplinary SC Physical Geography; Geology GA 087LD UT WOS:000240743000005 ER PT J AU Cloutis, EA Hawthorne, FC Mertzman, SA Krenn, K Craig, MA Marcino, D Methot, M Strong, J Mustard, JF Blaney, DL Bell, JF Vilas, F AF Cloutis, Edward A. Hawthorne, Frank C. Mertzman, Stanley A. Krenn, Katherine Craig, Michael A. Marcino, Dionne Methot, Michelle Strong, Johnathon Mustard, John F. Blaney, Diana L. Bell, James F., III Vilas, Faith TI Detection and discrimination of sulfate minerals using reflectance spectroscopy SO ICARUS LA English DT Review DE asteroids, composition; Europa; Mars, surface; meteorites; mineralogy; spectroscopy ID INFRARED-EMISSION SPECTROSCOPY; PLAYA EVAPORITE MINERALS; HYDRATED SALT MINERALS; IRON HYDROXY SULFATES; SOIL ANALOG MATERIALS; MU-M; SPECTRAL REFLECTANCE; FERRIC IRON; OMEGA/MARS EXPRESS; MARS SOIL AB A suite of sulfate minerals were characterized spectrally, compositionally, and structurally in order to develop spectral reflectance-compositional-structural relations for this group of minerals. Sulfates exhibit diverse spectral properties, and absorption-band assignments have been developed for the 0.3-26 mu m range. Sulfate absorption features can be related to the presence of transition elements, OH, H2O, and SO4 groups. The number, wavelength position, and intensity of these bands are a function of both composition and structure. Cation substitutions can affect the wavelength positions of all major absorption bands. Hydroxo-bridged Fe3+ results in absorption bands in the 0.43, 0.5, and 0.9 mu m regions, while the presence of Fe2+ results in absorption features in the 0.9-1.2 mu m interval. Fundamental S-O bending and stretching vibration absorption bands occur in the 8-10, 13-18, and 19-24 mu m regions (1000-1250, 550-770, and 420-530 cm(-1)). The most intense combinations and overtones of these fundamentals are found in the 4-5 mu m (2000-2500 cm(-1)) region. Absorption features seen in the 1.7-1.85 mu m interval are attributable to H-O-H/O-H bending and translation/rotation combinations, while bands in the 2.1-2.7 mu m regions can be attributed to H2O- and OH-combinations as well as overtones of S-O bending fundamentals. OH- and H2O-bearing sulfate spectra are fundamentally different from each other at wavelengths below similar to 6 mu m. Changes in H2O/OH content can shift S-O band positions due to change in bond lengths and structural rearrangement. Differences in absorption band wavelength positions enable discrimination of all the sulfate minerals used in this study in a number of wavelength intervals. Of the major absorption band regions, the 4-5 mu m region seems best for identifying and discriminating sulfates in the presence of other major rock-forming minerals. (c) 2006 Elsevier Inc. All rights reserved. C1 Univ Winnipeg, Dept Geog, Winnipeg, MB R3B 2E9, Canada. Univ Manitoba, Dept Geol Sci, Winnipeg, MB R3T 2N2, Canada. Franklin & Marshall Coll, Dept Geosci, Lancaster, PA 17604 USA. Brown Univ, Dept Geol Sci, Providence, RI 02912 USA. Jet Propuls Lab, Pasadena, CA 91009 USA. Cornell Univ, Dept Astron, Ithaca, NY 14853 USA. NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. RP Cloutis, EA (reprint author), Univ Winnipeg, Dept Geog, 515 Portage Ave, Winnipeg, MB R3B 2E9, Canada. EM e.cloutis@uwinnipeg.ca RI Hawthorne, Frank/F-6864-2011 OI Hawthorne, Frank/0000-0001-6405-9931 NR 177 TC 157 Z9 157 U1 2 U2 22 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 EI 1090-2643 J9 ICARUS JI Icarus PD SEP PY 2006 VL 184 IS 1 BP 121 EP 157 DI 10.1016/j.icarus.2006.04.003 PG 37 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 080KU UT WOS:000240247400007 ER PT J AU Klein, MJ Hofstadter, MD AF Klein, M. J. Hofstadter, M. D. TI Long-term variations in the microwave brightness temperature of the Uranus atmosphere SO ICARUS LA English DT Article DE Uranus; Uranus, atmosphere; atmospheres, dynamics; radio observations ID PHOTOMETRIC VARIABILITY; RADIO OBSERVATIONS; THERMAL STRUCTURE; DEEP ATMOSPHERE; NEPTUNE; SATURN; CM; VOYAGER-2; EMISSION; JUPITER AB We present a self-consistent, 36-year record of the disk-averaged radio brightness of Uranus at wavelengths near 3.5 cm. It covers nearly half a uranian year, and includes both equatorial and polar viewing geometries (corresponding to equinox and solstice, respectively). We find large (greater than 30 K) changes over this time span. In agreement with analyses made of more limited microwave data sets, our observations suggest the changes are not caused by geometric effects alone, and that temporal variations may exist in the deep uranian troposphere down to pressures of tens of bars. Our data also support an earlier suggestion that a rapid, planetary-scale change may have occurred in late 1993 and early 1994. The seasonal record presented here will be useful for constraining dynamical models of the deep atmosphere, and for interpreting observations made during Uranus' 2007 equinox passage. As part of a multi-wavelength observing campaign for this event, the Goldstone-Apple Valley Radio Telescope (GAVRT) project will continue to make frequent, single-dish observations near 3.5 cm. (c) 2006 Elsevier Inc. All rights reserved. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Hofstadter, MD (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr,Mail Stop 303-401, Pasadena, CA 91109 USA. EM michael.j.klein@jpl.nasa.gov; mark.d.hofstadter@jpl.nasa.gov NR 40 TC 7 Z9 7 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 SEP PY 2006 VL 184 IS 1 BP 170 EP 180 DI 10.1016/j.icarus.2006.04.012 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 080KU UT WOS:000240247400009 ER PT J AU Bauer, JM Grav, T Buratti, BJ Hicks, MD AF Bauer, James M. Grav, Tommy Buratti, Bonnie J. Hicks, Michael D. TI The phase curve of the irregular saturnian satellites: A possible method of physical classification SO ICARUS LA English DT Article DE Saturn satellites; satellites surfaces; photometry ID KUIPER-BELT OBJECTS; OUTER SOLAR-SYSTEM; PHOTOMETRIC PROPERTIES; OPPOSITION SURGE; MOON PHOEBE; CENTAURS; ANGLES; SPECTROSCOPY; ASTEROIDS; SURFACE AB During its 2005 January opposition, the saturnian system could be viewed at an unusually low phase angle. We surveyed a subset of Saturn's irregular satellites to obtain their true opposition magnitudes, or nearly so, down to phase angle values of 0.01 degrees. Combining our data taken at the Palomar 200-inch and Cerro Tololo Inter-American Observatory's 4-m Blanco telescope with those in the literature, we present the first phase curves for nearly half the irregular satellites originally reported by Gladman et al. [2001. Nature 412, 163-166], including Paaliaq (SXX), Siarnaq (SXXIX), Tarvos (SXXI), Ijiraq (SXXII), Albiorix (SXVI), and additionally Phoebe's narrowest angle brightness measured to date. We find centaur-like steepness in the phase curves or opposition surges in most cases with the notable exception of three, Albiorix and Tarvos, which are suspected to be of similar origin based on dynamical arguments, and Siarnaq. (c) 2006 Elsevier Inc. All rights reserved. C1 CALTECH, Jet Prop Lab, Palomar Observ, Pasadena, CA 91109 USA. Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. RP Bauer, JM (reprint author), CALTECH, Jet Prop Lab, Palomar Observ, 4800 Oak Grove Dr,Mail Stop 183-501, Pasadena, CA 91109 USA. EM bauer@scn.jpl.nasa.gov NR 58 TC 9 Z9 9 U1 0 U2 0 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 J9 ICARUS JI Icarus PD SEP PY 2006 VL 184 IS 1 BP 181 EP 197 DI 10.1016/j.icarus.2006.04.011 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 080KU UT WOS:000240247400010 ER PT J AU Shepard, MK Margot, JL Magri, C Nolan, MC Schlieder, J Estes, B Bus, SJ Volquardsen, EL Rivkin, AS Benner, LAM Giorgini, JD Ostro, SJ Busch, MW AF Shepard, Michael K. Margot, Jean-Luc Magri, Christopher Nolan, Michael C. Schlieder, Joshua Estes, Benjamin Bus, Schelte J. Volquardsen, Eric L. Rivkin, Andrew S. Benner, Lance A. M. Giorgini, Jon D. Ostro, Steven J. Busch, Michael W. TI Radar and infrared observations of binary near-Earth Asteroid 2002 CE26 SO ICARUS LA English DT Article DE asteroids; asteroids composition; asteroids surfaces; radar observations ID NEAR-EARTH ASTEROIDS; SPECTROGRAPH; OBJECTS; MODEL; SPEX AB We observed near-Earth Asteroid (NEA) 2002 CE26 in August and September 2004 using the Arecibo S-band (2380-MHz, 12.6-cm) radar and NASAs Infrared Telescope Facility (IRTF). Shape models obtained based on inversion of our delay-Doppler images show the asteroid to be 3.5 +/- 0.4 km in diameter and spheroidal; our corresponding nominal estimates of its visual and radar albedos are 0.07 and 0.24, respectively. Our IRTF spectrum shows the asteroid to be C-class with no evidence of hydration. Thermal models from the IRTF data provide a size and visual albedo consistent with the radar-derived estimate. We estimate the spin-pole to be within a few tens of degrees of lambda = 317 degrees, beta = -20 degrees. Our radar observations reveal a secondary approximately 0.3 km in diameter, giving this binary one of the largest size differentials of any known NEA. The secondary is in a near-circular orbit with period 15.6 +/- 0.1 h and a semi-major axis of 4.7 +/- 0.2 km. Estimates of the binary orbital pole and secondary rotation rate are consistent with the secondary being in a spin-locked equatorial orbit. The orbit corresponds to a primary mass of M = 1.95 +/- 0.25 x 10(13) kg, leading to a primary bulk density of rho = 0.9 + 0.5/-0.4 g cm(-3), one of the lowest values yet measured for a main-belt or near-Earth asteroid. (c) 2006 Elsevier Inc. All rights reserved. C1 Bloomsburg Univ Penn, Dept Geog & Geosci, Bloomsburg, PA 17815 USA. Bloomsburg Univ Penn, Dept Phys & Engn Technol, Bloomsburg, PA 17815 USA. Cornell Univ, Dept Astron, Ithaca, NY 14853 USA. Univ Maine, Farmington, ME 04938 USA. Natl Astron & Ionosphere Ctr, Arecibo Observ, Arecibo, PR 00612 USA. Univ Hawaii, Hilo, HI 96720 USA. Astron Inst, Hilo, HI 96720 USA. Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Shepard, MK (reprint author), Bloomsburg Univ Penn, Dept Geog & Geosci, 400 E 2nd St, Bloomsburg, PA 17815 USA. EM mshepard@bloomu.edu RI Margot, Jean-Luc/A-6154-2012; Nolan, Michael/H-4980-2012; Rivkin, Andrew/B-7744-2016 OI Margot, Jean-Luc/0000-0001-9798-1797; Nolan, Michael/0000-0001-8316-0680; Rivkin, Andrew/0000-0002-9939-9976 NR 36 TC 26 Z9 28 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 SEP PY 2006 VL 184 IS 1 BP 198 EP 210 DI 10.1016/j.icarus.2006.04.019 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 080KU UT WOS:000240247400011 ER PT J AU Dello Russo, N Mumma, MJ DiSanti, MA Magee-Sauer, K Gibb, EL Bonev, BP McLean, IS Xu, LH AF Dello Russo, Neil Mumma, Michael J. DiSanti, Michael A. Magee-Sauer, Karen Gibb, Erika L. Bonev, Boncho P. McLean, I. S. Xu, Li-Hong TI A high-resolution infrared spectral survey of Comet C/1999 H1 Lee SO ICARUS LA English DT Review DE comets; infrared; observations; spectroscopy ID O1 HALE-BOPP; FREQUENCY LASER SPECTROSCOPY; 1ST ABSORPTION-BAND; IKS-VEGA EXPERIMENT; WATER PRODUCTION; MU-M; EMISSION FEATURE; B2 HYAKUTAKE; NU-3 BAND; FLUORESCENCE EFFICIENCIES AB We obtained high-resolution (lambda/Delta lambda similar to 25,000) spectra of Comet C/1999 H1 (Lee) on UT 1999 August 19.6 and 21.6 using the cross-dispersed Near InfraRed SPECtrometer (NIRSPEC) at the Keck Observatory atop Mauna Kea, HI. Here we present spectra of Comet Lee between 2.874 and 3.701 mu m (3479-2702 cm(-1)) representing the most complete high-resolution infrared survey of a comet to date in this wavelength region. Using published line lists and laboratory spectra we have identified 444 of the 545 distinct emission features present in these spectra. We have tabulated the rest frequencies, assignments, relative intensities, and signal-to-noise ratios of all detected emissions. In addition to gaining insights into the chemistry of Comet Lee, this survey provides a valuable tool for planning future high-resolution infrared observations of comets and other astronomical targets, and for retrospective comparison to existing high-resolution infrared datasets. (c) 2006 Elsevier Inc. All rights reserved. C1 Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA. NASA, Goddard Space Flight Ctr, Solar Syst Explorat Div, Planetary Syst Lab, Greenbelt, MD 20771 USA. Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA. Rowan Univ, Dept Chem & Phys, Glassboro, NJ 08028 USA. Univ Missouri, Dept Phys & Astron, St Louis, MO 63121 USA. Univ Toledo, Dept Phys & Astron, Ritter Astronphys Res Ctr, Toledo, OH 43606 USA. Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA. Univ New Brunswick, Dept Phys Sci, Ctr Laser Atom & Mol Sci, St John, NB E2L 4L5, Canada. RP Dello Russo, N (reprint author), Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA. EM neil.dello.russo@jhuapl.edu RI mumma, michael/I-2764-2013; Xu, Li-Hong/J-5095-2015; Magee-Sauer, Karen/K-6061-2015; Dello Russo, Neil/G-2727-2015 OI Magee-Sauer, Karen/0000-0002-4979-9875; Dello Russo, Neil/0000-0002-8379-7304 NR 180 TC 33 Z9 33 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 SEP PY 2006 VL 184 IS 1 BP 255 EP 276 DI 10.1016/j.icarus.2006.04.020 PG 22 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 080KU UT WOS:000240247400015 ER PT J AU Harmon, JK Nolan, MC Margot, JL Campbell, DB Benner, LAM Giorgini, JD AF Harmon, J. K. Nolan, M. C. Margot, J. -L. Campbell, D. B. Benner, L. A. M. Giorgini, J. D. TI Radar observations of Comet P/2005 JQ5 (Catalina) SO ICARUS LA English DT Article DE comets; radar observations; comets, nucleus; comets, dust ID DUST TRAILS AB Arecibo radar observations of Comet P/2005 JQ5 (Catalina) have produced the first delay-Doppler images of a comet nucleus and the first radar detection of large-grain ejection from a Jupiter-family comet. The nucleus is small (1.4 km diameter), rough, and rapidly rotating. The large (> cm) grains have low velocities (similar to 1 m/s) and a low production rate. (c) 2006 Elsevier Inc. All rights reserved. C1 Natl Astron & Ionosphere Ctr, Arecibo Observ, Arecibo, PR 00612 USA. Cornell Univ, Dept Astron, Ithaca, NY 14853 USA. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Harmon, JK (reprint author), Natl Astron & Ionosphere Ctr, Arecibo Observ, Arecibo, PR 00612 USA. EM harmon@naic.edu RI Margot, Jean-Luc/A-6154-2012; Nolan, Michael/H-4980-2012 OI Margot, Jean-Luc/0000-0001-9798-1797; Nolan, Michael/0000-0001-8316-0680 NR 23 TC 8 Z9 8 U1 0 U2 0 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 J9 ICARUS JI Icarus PD SEP PY 2006 VL 184 IS 1 BP 285 EP 288 DI 10.1016/j.icarus.2006.05.014 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 080KU UT WOS:000240247400017 ER PT J AU Maunder, MN Sibert, JR Fonteneau, A Hampton, J Kleiber, P Harley, SJ AF Maunder, Mark N. Sibert, John R. Fonteneau, Alain Hampton, John Kleiber, Pierre Harley, Shelton J. TI Interpreting catch per unit effort data to assess the status of individual stocks and communities SO ICES JOURNAL OF MARINE SCIENCE LA English DT Article DE cpue; ecosystem; fisheries management; Pacific Ocean; stock assessment; tuna ID LONG-TERM FLUCTUATIONS; COD GADUS-MORHUA; FISHERIES MANAGEMENT; BLUEFIN TUNA; EXPLOITED ECOSYSTEMS; REFERENCE POINTS; DYNAMIC-MODELS; TROPICAL TUNAS; PACIFIC-OCEAN; ATLANTIC AB Despite being one of the most common pieces of information used in assessing the status of fish stocks, relative abundance indices based on catch per unit effort (cpue) data are notoriously problematic. Raw cpue is seldom proportional to abundance over a whole exploitation history and an entire geographic range, because numerous factors affect catch rates. One of the most commonly applied fisheries analyses is standardization of cpue data to remove the effect of factors that bias cpue as an index of abundance. Even if cpue is standardized appropriately, the resulting index of relative abundance, in isolation, provides limited information for management advice or about the effect of fishing. In addition, cpue data generally cannot provide information needed to assess and manage communities or ecosystems. We discuss some of the problems associated with the use of cpue data and some methods to assess and provide management advice about fish populations that can help overcome these problems, including integrated stock assessment models, management strategy evaluation, and adaptive management. We also discuss the inappropriateness of using cpue data to evaluate the status of communities. We use tuna stocks in the Pacific Ocean as examples. (c) 2006 International Council for the Exploration of the Sea. Published by Elsevier Ltd. All rights reserved. C1 InterAmer Trop Tuna Commiss, La Jolla, CA 92037 USA. Univ Hawaii, Pelag Fisheries Res Program, Honolulu, HI 96822 USA. Ctr Rech Halieut Mediterraneenne & Trop, F-34203 Sete, France. Secretariat Pacific Community, Ocean Fisheries Programme, Noumea, New Caledonia. NOAA, Natl Marine Fisheries Serv, Pacific Isl Fisheries Sci Ctr, Honolulu, HI 96822 USA. Minist Fisheries, Wellington, New Zealand. RP Maunder, MN (reprint author), InterAmer Trop Tuna Commiss, 8604 La Jolla Shores Dr, La Jolla, CA 92037 USA. EM nunaunder@iattc.org NR 85 TC 158 Z9 167 U1 6 U2 66 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 1054-3139 J9 ICES J MAR SCI JI ICES J. Mar. Sci. PD SEP PY 2006 VL 63 IS 8 BP 1373 EP 1385 DI 10.1016/j.icejms.2006.05.008 PG 13 WC Fisheries; Marine & Freshwater Biology; Oceanography SC Fisheries; Marine & Freshwater Biology; Oceanography GA 084OP UT WOS:000240543100001 ER PT J AU Qu, ZH Wang, J Plaisted, CE Hull, RA AF Qu, Zhihua Wang, Jing Plaisted, Clinton E. Hull, Richard A. TI Global-stabilizing near-optimal control design for nonholonomic chained systems SO IEEE TRANSACTIONS ON AUTOMATIC CONTROL LA English DT Article DE near-optimal control; nonholonomic chained systems; output feedback; state feedback; tracking control ID NONLINEAR CONTROL-SYSTEMS; TRACKING CONTROL; MOBILE ROBOTS; EXPONENTIAL STABILIZATION; CONTROL LAWS; FORM SYSTEMS; POWER FORM; FEEDBACK AB It is well known that a nonlinear optimal control requires the solution to a two-point boundary value problem or to a nonlinear partial differential equation and that such a solution can only be obtained off line by numerical iteration. In this paper, a new and near-optimal control design framework is proposed for controlling any nonholonomic system in the chained form. The proposed design is based upon thorough study of uniform complete controllability of the corresponding linear time varying nominal system. It is shown that, no matter whether the first component u(1d)(t) of reference input vector is uniformly nonvanishing or simply nonconvergent to zero or vanishing or identically zero, uniform complete controllability of the (nominal) system can be recovered by employing the proposed time-folding/unfolding technique. Upon establishing the common property of uniform complete controllability, the proposed framework can be used to design both trajectory tracking control and regulation control in a systematic and unified manner. Using duality, uniform complete observability can also be established, a closed-form and exponentially convergent observer can be synthesized, and the controls designed using the proposed framework can be either state-feedback or output-feedback. The tracking controls are designed using the same three-step process. That is, design of the proposed controls starts with optimal control solutions to two linear nominal subsystems, one time-invariant and the other time varying. The two solutions combined together render a globally stabilizing suboptimal control for the overall system. Then, the optimality condition is invoked to determine the distance between the suboptimal control and the optimal one. Consequently, an improved control can be obtained by introducing a nonlinear additive control term in such a way that the distance aforementioned is minimized as much as possible in closed form. An example is used to show that regulation control can be designed similarly. All the controls designed are in simple closed forms and hence real-time implementable, they are time varying and smooth, globally and exponentially/asymptotically stabilizing, and they are near optimal since their closeness to the optimal control (attainable only offline) can be measured, monitored on line, and has been minimized. C1 Univ Cent Florida, Dept Elect & Comp Engn, Orlando, FL 32816 USA. NASA, ELV Mission Anal Branch, AI Solut Inc, Kennedy Space Ctr, FL 32899 USA. SAIC, Orlando, FL 32801 USA. RP Qu, ZH (reprint author), Univ Cent Florida, Dept Elect & Comp Engn, Orlando, FL 32816 USA. EM qu@mail.ucf.edu; jwang@pegasus.cc.ucf.edu NR 39 TC 30 Z9 36 U1 1 U2 5 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 0018-9286 J9 IEEE T AUTOMAT CONTR JI IEEE Trans. Autom. Control PD SEP PY 2006 VL 51 IS 9 BP 1440 EP 1456 DI 10.1109/TAC.2006.880965 PG 17 WC Automation & Control Systems; Engineering, Electrical & Electronic SC Automation & Control Systems; Engineering GA 085BU UT WOS:000240579000003 ER PT J AU Shin, JY Belcastro, CM AF Shin, Jong-Yeob Belcastro, Christine M. TI Performance analysis on fault tolerant control system SO IEEE TRANSACTIONS ON CONTROL SYSTEMS TECHNOLOGY LA English DT Article DE aircraft; control systems; fault tolerant; highly maneuverable aircraft technology (HiMAT) vehicle; linear matrix inequality; linear parameter varying system ID ACCOMMODATION; FAILURE AB In a fault tolerant control (FTC) system, a parameter varying FTC law is reconfigured according to fault parameters estimated by fault detection and isolation (FDI) modules. FDI modules require some time to detect fault occurrences in aero-vehicle dynamics. In this brief, an FTC analysis framework is provided to calculate the upper bound of an induced-L-2 norm of an FTC system in the presence of false identification and detection time delay. The upper bound is written as a function of a duration time interval and exponential decay rates and has been used to determine which FTC law produces less performance degradation (tracking error) due to false identification. The analysis framework is applied for an FTC system of a highly maneuverable aircraft technology (HiMAT) vehicle. C1 Natl Inst Aerosp, Hampton, VA 23666 USA. NASA, Langley Res Ctr, Dynam Syst & Control Branch, Aircraft Guidance & Control, Hampton, VA 23681 USA. RP Shin, JY (reprint author), Natl Inst Aerosp, Hampton, VA 23666 USA. EM shinjy@nianet.org NR 11 TC 17 Z9 20 U1 0 U2 5 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 SEP PY 2006 VL 14 IS 5 BP 920 EP 925 DI 10.1109/TCST.2006.876911 PG 6 WC Automation & Control Systems; Engineering, Electrical & Electronic SC Automation & Control Systems; Engineering GA 072YQ UT WOS:000239709600012 ER PT J AU Franceschetti, G Iodice, A Perna, S Riccio, D AF Franceschetti, Giorgio Iodice, Antonio Perna, Stefano Riccio, Daniele TI SAR sensor trajectory deviations: Fourier domain formulation and extended scene simulation of raw signal SO IEEE TRANSACTIONS ON GEOSCIENCE AND REMOTE SENSING LA English DT Article DE motion compensation; simulation; synthetic aperture radar (SAR) ID AIRBORNE SAR; MOTION COMPENSATION; ACCURACY; IMAGES AB Synthetic aperture radar (SAR) raw signal simulation is a useful tool for SAR system design, mission planning, processing algorithm testing, and inversion algorithm design. A two-dimensional (2-D) Fourier domain SAR raw signal simulator, exploiting the efficiency of fast Fourier transform algorithms, has been presented some years ago and is able to generate the raw signal corresponding to extended scenes. However, it cannot account for the effects of sensor trajectory deviations with respect to the nominal straight-line path. This paper explores the possibility of extending the efficient Fourier domain simulation approach to the case of sensor trajectory deviations, which is more realistic for airborne SAR systems. We first of all obtain a general and compact Fourier domain formulation of the SAR raw signal in the presence of arbitrary trajectory deviations, and show that in this general case no efficient simulation scheme can be devised. However, we demonstrate that, if a narrow beam and slow trajectory deviation assumption is made, a full 2-D Fourier domain simulation can be used. This approach can be applied only to some SAR systems and/or trajectory deviations, but it has the advantage that processing time is practically not increased with respect to the nominal trajectory case. The validity limits of the approach are analytically evaluated. Some simulation results are finally presented in order to verify the effectiveness of the proposed simulation scheme. In another paper, which is the second part of this work, it will be shown that the narrow beam-slow deviation assumption can be relaxed, at the expense of computation efficiency, if a one-dimensional azimuth Fourier domain processing followed by a range time-domain integration is used. C1 Univ Naples Federico II, Dipartimento Ingn Elettron & Telecomun, I-80125 Naples, Italy. Univ Calif Los Angeles, Los Angeles, CA 90095 USA. Jet Prop Lab, Pasadena, CA 91109 USA. Ist Rilevamento Elettromagnet Ambiente, I-80124 Naples, Italy. RP Franceschetti, G (reprint author), Univ Naples Federico II, Dipartimento Ingn Elettron & Telecomun, I-80125 Naples, Italy. EM gfrance@unina.it; iodice@unina.it; steperna@unina.it; daniele.riccio@unina.it OI Iodice, Antonio/0000-0001-6173-3601; Perna, Stefano/0000-0002-3951-5816 NR 17 TC 43 Z9 53 U1 2 U2 9 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855 USA SN 0196-2892 J9 IEEE T GEOSCI REMOTE JI IEEE Trans. Geosci. Remote Sensing PD SEP PY 2006 VL 44 IS 9 BP 2323 EP 2334 DI 10.1109/TGRS.2006.873206 PG 12 WC Geochemistry & Geophysics; Engineering, Electrical & Electronic; Remote Sensing; Imaging Science & Photographic Technology SC Geochemistry & Geophysics; Engineering; Remote Sensing; Imaging Science & Photographic Technology GA 079HT UT WOS:000240167200001 ER PT J AU Manizade, KE Spinhirne, JD Lancaster, RS AF Manizade, Kathrine E. Spinhirne, James D. Lancaster, Redgie S. TI Stereo cloud heights from multispectral IR imagery via region-of-interest segmentation SO IEEE TRANSACTIONS ON GEOSCIENCE AND REMOTE SENSING LA English DT Article DE clouds; image segmentation; infrared imaging; remote sensing; stereo vision ID SHUTTLE MISSION STS-85; OCTOBER 1986 FIRE; OPTICAL-PROPERTIES; RADIOMETER; WINDOW AB Multispectral thermal imagery acquired from low Earth orbit was used to develop a method of cloud-height determination that applies image brightness temperature histograms and region-of-interest (ROI) image segmentation as a processing step prior to stereo-height retrieval. The National Aeronautics and Space Administration's Infrared Spectral Imaging Radiometer (ISIR) acquired all imagery during the August 1997 STS-85 mission of the Space Shuttle Discovery. ISIR, the first Earth-observing spectroradiometer to employ an uncooled large-format microbolometer-array focal plane, provided continuous coverage in four spectral bands along track in an 80-km-wide swath. ROI segmentation created binary cloud masks ranging over brightness temperatures in the imagery for which the parallax was determined by a two-dimensional correlation method, allowing stereo heights to be determined using the standard parallax equations. A subpixel parallax algorithm allowed stereo heights to be determined with a precision of roughly +/- 0.39 km for clouds in the observed altitude range of 0.5-10 km. C1 Sci Syst & Applicat Inc, Lanham, MD 20706 USA. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Univ Maryland Baltimore Cty, Goddard Earth Sci & Technol Ctr, Baltimore, MD 21250 USA. RP Manizade, KE (reprint author), Sci Syst & Applicat Inc, Lanham, MD 20706 USA. EM manizade@comcast.net; jspin@virl.gsfc.nasa.gov; lancaster@virl.gsfc.nasa.gov NR 16 TC 7 Z9 7 U1 0 U2 4 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855 USA SN 0196-2892 J9 IEEE T GEOSCI REMOTE JI IEEE Trans. Geosci. Remote Sensing PD SEP PY 2006 VL 44 IS 9 BP 2481 EP 2491 DI 10.1109/TGRS.2006.873339 PG 11 WC Geochemistry & Geophysics; Engineering, Electrical & Electronic; Remote Sensing; Imaging Science & Photographic Technology SC Geochemistry & Geophysics; Engineering; Remote Sensing; Imaging Science & Photographic Technology GA 079HT UT WOS:000240167200017 ER PT J AU Enzer, DG Klipstein, WM AF Enzer, Daphna G. Klipstein, William M. TI Characterization of light shift below 10(-15) in a cesium fountain frequency standard operated without the use of mechanical shutters SO IEEE TRANSACTIONS ON ULTRASONICS FERROELECTRICS AND FREQUENCY CONTROL LA English DT Article ID LASER COOLED CLOCKS AB We characterize the light shift in the interaction region of a laser-cooled frequency standard and demonstrate an approach for its mitigation without the use of mechanical shutters. The light shift is confirmed to be below 10(-15) and expected to be orders of magnitude lower. This technique makes use of a master-slave laser configuration where cutting the injection power to a slave laser causes it to lase at its free-running wavelength, often two or more nanometers off from the atomic resonance. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Enzer, DG (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM Daphna.G.Enzer@jpl.nasa.gov NR 10 TC 3 Z9 3 U1 0 U2 5 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 0885-3010 J9 IEEE T ULTRASON FERR JI IEEE Trans. Ultrason. Ferroelectr. Freq. Control PD SEP PY 2006 VL 53 IS 9 BP 1564 EP 1569 DI 10.1109/TUFFC.2006.1678184 PG 6 WC Acoustics; Engineering, Electrical & Electronic SC Acoustics; Engineering GA 076BM UT WOS:000239932000006 PM 16964906 ER PT J AU Ellsworth, D Green, B Henze, C Moran, P Sandstrom, T AF Ellsworth, David Green, Bryan Henze, Chris Moran, Patrick Sandstrom, Timothy TI Concurrent visualization in a production supercomputing environment SO IEEE TRANSACTIONS ON VISUALIZATION AND COMPUTER GRAPHICS LA English DT Article; Proceedings Paper CT IEEE Visualization Conference (Vis 2006)/IEEE Symposium on Information Visualization (InfoVis 2006) CY OCT 29-NOV 03, 2006 CL Baltimore, MD SP IEEE DE supercomputing; concurrent visualization; interactive visual computing; time-varying data; high temporal resolution visualization; GEOS4 global climate model; hurricane visualization; ECCO; ocean modeling AB We describe a concurrent visualization pipeline designed for operation in a production supercomputing environment. supercomputer for a massively parallel forecast model (GEOS4). During the 2005 Atlantic hurricane season, GEOS4 was run 4 times a day under tight time constraints so that its output could be included in an ensemble prediction that was made available to forecasters at the National Hurricane Center. Given this time-critical context, we designed a configurable concurrent pipeline to visualize multiple global fields without significantly affecting the runtime model performance or reliability. We use MPEG compression of the accruing images to facilitate live low-bandwidth distribution of multiple visualization streams to remote sites. We also describe the use of our concurrent visualization framework with a global ocean circulation model, which provides a 864-fold increase in the temporal resolution of practically achievable animations. In both the atmospheric and oceanic circulation models, the application scientists gained new insights into their model dynamics, due to the high temporal resolution animations attainable. C1 NASA, Ames Res Ctr, AMTI, Washington, DC 20546 USA. RP Ellsworth, D (reprint author), NASA, Ames Res Ctr, AMTI, 300 E St SW, Washington, DC 20546 USA. EM ellswort@nas.nasa.gov; bgreen@nas.nasa.gov; chenze@nas.nasa.gov; patrick.j.moran@nasa.gov; sandstro@nos.naso.gov NR 18 TC 10 Z9 10 U1 0 U2 0 PU IEEE COMPUTER SOC PI LOS ALAMITOS PA 10662 LOS VAQUEROS CIRCLE, PO BOX 3014, LOS ALAMITOS, CA 90720-1314 USA SN 1077-2626 EI 1941-0506 J9 IEEE T VIS COMPUT GR JI IEEE Trans. Vis. Comput. Graph. PD SEP-OCT PY 2006 VL 12 IS 5 BP 997 EP 1004 DI 10.1109/TVCG.2006.128 PG 8 WC Computer Science, Software Engineering SC Computer Science GA 096NE UT WOS:000241383300044 PM 17080827 ER PT J AU Yang, HC Simon, MK Alouini, MS AF Yang, Hong-Chuan Simon, Marvin K. Alouini, Mohamed-Slim TI Scan and wait combining (SWC): A switch and examine strategy with a performance-delay tradeoff SO IEEE TRANSACTIONS ON WIRELESS COMMUNICATIONS LA English DT Article; Proceedings Paper CT 1st IEEE Intenational Symposium on Control, Communications and Signal Processing (ISCCSP 2004) CY MAR 21-24, 2004 CL Hammamet, TUNISIA SP IEEE, European Soc Signal Proc, Minist Enseignement Super Rech Sci Technol, Minist Technol CommunTransport, Minist Commerce Tourisme Artisanat Tunisia DE fading channels; diversity techniques; switched diversity; and performance analysis ID DIVERSITY SYSTEMS; FADING CHANNELS; OPTIMIZATION; RAYLEIGH AB This paper proposes and analyzes an alternative form of switch and examine combining, namely one that waits for a channel coherence time if all the available diversity paths fail to meet a predetermined minimum quality requirement. This scanning through the available diversity paths followed by waiting process is repeated indefinitely until a path with an acceptable quality is found. The performance of the resulting, "scan and wait" combining (SWC) scheme is studied in terms of its average probability of error and ergodic capacity. The paper looks also into (i) the delay associated with SWC by deriving the statistics of the waiting time needed before satisfactory transmission occurs and (ii) the underlying complexity by studying the statistics of the number of diversity paths estimated per channel access. Selected numerical examples show that, for a fixed average number of channel estimates per channel access, SWC outperforms traditional diversity combining schemes at the expense of a negligible time delay. C1 Univ Victoria, Dept Elect & Comp Engn, Victoria, BC V8W 3P6, Canada. JPL, Pasadena, CA 91109 USA. TAMU, Dept Elect Engn, Doha, Qatar. RP Yang, HC (reprint author), Univ Victoria, Dept Elect & Comp Engn, Victoria, BC V8W 3P6, Canada. EM hyang@ece.uvic.ca; marvin.k.simon@jpl.nasa.gov; alouini@qatar.tamu.edu NR 16 TC 14 Z9 14 U1 0 U2 2 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855 USA SN 1536-1276 J9 IEEE T WIREL COMMUN JI IEEE Trans. Wirel. Commun. PD SEP PY 2006 VL 5 IS 9 BP 2477 EP 2483 DI 10.1109/TWC.2006.04369 PG 7 WC Engineering, Electrical & Electronic; Telecommunications SC Engineering; Telecommunications GA 091TG UT WOS:000241050600024 ER PT J AU Pikuta, EV Hoover, RB Bei, AK Marsic, D Whitman, WB Krader, PE Tang, J AF Pikuta, Elena V. Hoover, Richard B. Bei, Asim K. Marsic, Damien Whitman, William B. Krader, Paul E. Tang, Jane TI Trichococcus patagoniensis sp nov., a facultative anaerobe that grows at -5 degrees C, isolated from penguin guano in Chilean Patagonia SO INTERNATIONAL JOURNAL OF SYSTEMATIC AND EVOLUTIONARY MICROBIOLOGY LA English DT Article ID DNA HYBRIDIZATION; LACTOSPHAERA-PASTEURII; RUMINOCOCCUS-PASTEURII; RENATURATION RATES; SEQUENCE ALIGNMENT; RIBOSOMAL-RNA; MONO LAKE; GEN-NOV; BACTERIA; ACID AB A novel, extremely psychrotolerant, facultative anaerobe, strain PmagG1(T), was isolated from guano of Magellanic penguins (Spheniscus magellanicus) collected in Chilean Patagonia. Gram-variable, motile cocci with a diameter of 1.3-2.0 mu m were observed singularly or in pairs, short chains and irregular conglomerates. Growth occurred within the pH range 6.0-10.0, with optimum growth at pH 8.5. The temperature range for growth of the novel isolate was from -5 to 35 degrees C, with optimum growth at 28-30 degrees C. Strain PmagG1(T) did not require NaCl, as growth was observed in the presence of 0-6.5% NaCl with optimum growth at 0-5% (w/v). Strain PmagG1(T) was a catalase-negative chemo-organoheterotroph that used sugars and some organic acids as substrates. The metabolic end products were lactate, formate, acetate, ethanol and CO2. Strain PmagG1(T) was sensitive to ampicillin, tetracycline, chloramphenicol, rifampicin, kanamycin and gentamicin. The G + C content of its genomic DNA was 45.8 mol% 16S rRNA gene sequence analysis showed 100% similarity of strain PmagG1(T) with Trichococcus collinsii ATCC BAA-296(T), but DNA-DNA hybridization between them demonstrated relatedness values of < 45 +/- 1 %. Another phylogenetically closely related species, Trichococcus pasteurii, showed 99.85% similarity by 16S rRNA sequencing and DNA-DNA hybridization showed relatedness values of 47 +/- 1.5 %. Based on genotypic and phenotypic characteristics, the novel species Trichococcus patagoniensis sp. nov. is proposed, with strain PmagG1(T) (= ATCC BAA-756(T) = JCM 12176(T) = CIp 108035(T)) as the type strain. C1 NASA, NSSTC, Astrobiol Lab, Huntsville, AL 35805 USA. Univ Alabama, Dept Biol, Birmingham, AL 35294 USA. Univ Alabama, Struct Biol Lab, Huntsville, AL 35899 USA. Univ Georgia, Dept Microbiol, Athens, GA 30602 USA. Amer Type Culture Collect, Manassas, VA 20110 USA. Mitretek Syst, Falls Church, VA 22042 USA. RP Pikuta, EV (reprint author), NASA, NSSTC, Astrobiol Lab, VP-62,320 Sparkman Dr, Huntsville, AL 35805 USA. EM elenapikuta@hotmail.com; Richard.Hoover@NASA.GOV RI Marsic, Damien/A-1087-2009 OI Marsic, Damien/0000-0003-0847-8095 NR 31 TC 26 Z9 27 U1 0 U2 5 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 SEP PY 2006 VL 56 BP 2055 EP 2062 DI 10.1099/ijs.0.64225-0 PN 9 PG 8 WC Microbiology SC Microbiology GA 088AI UT WOS:000240783500005 PM 16957099 ER PT J AU Sherry, L Fennell, K Feary, M Polson, P AF Sherry, Lance Fennell, Karl Feary, Micheal Polson, Peter TI Human-computer interaction analysis of flight management system messages SO JOURNAL OF AIRCRAFT LA English DT Article AB Researchers have identified low proficiency in pilot response to flight management system error messages and have documented pilot perceptions that the messages contribute to the overall difficulty in learning and using the flight management system. It is well known that sharp reductions in pilot proficiency occur when pilots are asked to perform tasks that are time-critical, occur very infrequently, and are not guided by salient visual cues on the user-interface. This paper describes the results of an analysis of the pilot human-computer interaction required to respond to 67 flight management system error messages from a representative modern flight management system. Thirty-six percent of the messages require prompt pilot response, occur very infrequently, and are not guided by visual cues. These results explain, in part, issues with pilot proficiency, and demonstrate the need for deliberate design of the messages to account for the properties of human-computer interaction. Guidelines for improved training and design of the error messages are discussed. C1 San Jose State Univ, Res Fdn, NASA Ames Res Ctr, Moffett Field, CA 94035 USA. United Airlines, Denver, CO 80207 USA. NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. Univ Colorado, Boulder, CO 80309 USA. RP Sherry, L (reprint author), San Jose State Univ, Res Fdn, NASA Ames Res Ctr, Moffett Field, CA 94035 USA. NR 21 TC 2 Z9 2 U1 0 U2 3 PU AMER INST AERONAUT ASTRONAUT PI RESTON PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA SN 0021-8669 J9 J AIRCRAFT JI J. Aircr. PD SEP-OCT PY 2006 VL 43 IS 5 BP 1372 EP 1376 DI 10.2514/1.20026 PG 5 WC Engineering, Aerospace SC Engineering GA 100EH UT WOS:000241650100016 ER PT J AU Rossow, VJ AF Rossow, Vernon J. TI Vortex-free flight corridors for aircraft executing compressed landing operations SO JOURNAL OF AIRCRAFT LA English DT Article ID WAKES AB A factor that limits airport arrival and departure rates is the need to wait between operations for the wake vortices of preceding aircraft to decay to a safe level. As airport traffic demand increases, creative methods will be needed to overcome the limitations caused by the hazard posed by vortex wakes so that airport capacities can be safely increased. The problem addressed here is the design of vortex-free trajectories for aircraft as they fly from their cruise altitudes down to their final approach paths and to a landing. The guidelines presented recommend that the flight path of each aircraft in a group executing nearly simultaneous landings be spaced far enough apart laterally along organized flight paths so that the vortex wakes of preceding aircraft will not intrude into the airspace to be used by following aircraft. An example is presented as to how a combination of straight lines and circular arcs is able to provide each aircraft in a group with a vortex-free trajectory for nearly simultaneous landings on a set of closely spaced parallel runways. Although the guidelines are described for aircraft on approach,the concepts presented are also applicable to departure, and to en route operations. C1 NASA, Ames Res Ctr, Aviat Syst Div, Moffett Field, CA 94035 USA. RP Rossow, VJ (reprint author), NASA, Ames Res Ctr, Aviat Syst Div, Mail Stop N210-10, Moffett Field, CA 94035 USA. NR 19 TC 5 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 0021-8669 J9 J AIRCRAFT JI J. Aircr. PD SEP-OCT PY 2006 VL 43 IS 5 BP 1424 EP 1428 DI 10.2514/1.21614 PG 5 WC Engineering, Aerospace SC Engineering GA 100EH UT WOS:000241650100023 ER PT J AU Rouse, M Ambur, DR Dopker, B Shah, B AF Rouse, Marshall Ambur, Damodar R. Dopker, Bernard Shah, Bharat TI Response of composite fuselage sandwich side panels subjected to internal pressure and axial tension SO JOURNAL OF AIRCRAFT LA English DT Article AB An experimental and analytical study on the structural behavior of two carbon fiber reinforced plastic composite sandwich fuselage side panels for a transport aircraft is presented. Each panel has two window cutouts and three frames and uses a distinctly different structural concept. These panels have been evaluated with internal-pressure and axial tension load loading conditions. One of the sandwich panels was tested with the middle frame removed to demonstrate the suitability of this two-frame design for supporting the prescribed biaxial loading conditions with twice the initial frame spacing. A damage tolerance study was conducted on the two-frame panel by cutting a notch in the panel that originated at the edge of a cutout and extended in the panel hoop direction through the window-belt area. This panel with a notch was tested in a combined-load condition. Both sandwich panel designs successfully satisfied all desired load requirements in the experimental part of the study, and experimental results from the two-frame panel with and without damage are fully explained by the analytical results. The results of this study-suggest that there is potential for using sandwich structural concepts with greater than usual frame spacing to further reduce aircraft fuselage structural weight. C1 NASA, Langley Res Ctr, Mech Struct & Mat Branch, Hampton, VA 23681 USA. NASA, Glenn Res Ctr, Mat & Struc Div, Cleveland, OH 44135 USA. Boeing Commercial Airplane Co, Technol & Prod Dev Grp, Seattle, WA 98124 USA. Lockheed Martin Aeronaut Syst Co, Adv Struct & Mat Div, Marietta, GA USA. RP Rouse, M (reprint author), NASA, Langley Res Ctr, Mech Struct & Mat Branch, Hampton, VA 23681 USA. NR 3 TC 1 Z9 1 U1 3 U2 5 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 SEP-OCT PY 2006 VL 43 IS 5 BP 1440 EP 1447 DI 10.2514/1.22397 PG 8 WC Engineering, Aerospace SC Engineering GA 100EH UT WOS:000241650100026 ER PT J AU Carter, MB Campbell, RL Pendergraft, OC Friedman, DM Serrano, L AF Carter, Melissa B. Campbell, Richard L. Pendergraft, Odis C., Jr. Friedman, Douglas M. Serrano, Leonel TI Designing and testing a blended wing body with boundary-layer ingestion nacelles SO JOURNAL OF AIRCRAFT LA English DT Article; Proceedings Paper CT AIAA 43rd Aerospace Sciences Meeting and Exhibit CY JAN 10-13, 2005 CL Reno, NV SP AIAA AB A knowledge-based aerodynamic design method coupled with an unstructured grid Navier-Stokes flow solver was used to improve the propulsion/airframe integration for a blended wing body with boundary-layer ingestion nacelles. A new zonal design capability was used that significantly reduced the time required to achieve a successful design for each nacelle and the elevon between them. A wind-tunnel model was built with interchangeable parts reflecting the baseline and redesigned configurations and tested in the National Transonic Facility. Most of the testing was done at the cruise design conditions (Mach number of 0.85, Reynolds number of 75 million). In general, the predicted improvements in forces and moments as well as the changes in wing pressures between the baseline and redesign were confirmed by the wind-tunnel results. The effectiveness of elevons between the nacelles was also predicted surprisingly well considering the crudeness in the modeling of the control surfaces in the flow code. C1 NASA, Langley Res Ctr, Configurat Aerodynam Branch, Hampton, VA 23681 USA. Boeing Phantom Works, Huntington Beach, CA 92647 USA. RP Carter, MB (reprint author), NASA, Langley Res Ctr, Configurat Aerodynam Branch, MS 499, Hampton, VA 23681 USA. NR 25 TC 5 Z9 7 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 SEP-OCT PY 2006 VL 43 IS 5 BP 1479 EP 1489 DI 10.2514/1.22765 PG 11 WC Engineering, Aerospace SC Engineering GA 100EH UT WOS:000241650100030 ER PT J AU Turner, RT Lotinun, S Hefferan, TE Morey-Holton, E AF Turner, Russell T. Lotinun, Sutada Hefferan, Theresa E. Morey-Holton, Emily TI Disuse in adult male rats attenuates the bone anabolic response to a therapeutic dose of parathyroid hormone SO JOURNAL OF APPLIED PHYSIOLOGY LA English DT Article DE bone anabolic; aging; bone remodeling; exercise ID GROWTH-FACTOR-I; OVARIECTOMIZED RATS; POSTMENOPAUSAL WOMEN; MINERAL DENSITY; SIMULATED WEIGHTLESSNESS; CANCELLOUS BONE; MESSENGER-RNA; CORTICAL BONE; OSTEOPOROSIS; ESTROGEN AB Disuse in adult male rats attenuates the bone anabolic response to a therapeutic dose of parathyroid hormone. J Appl Physiol 101: 881-886, 2006. First published May 4, 2006; doi:10.1152/japplphysiol.01622.2005.-Intermittent treatment with parathyroid hormone (PTH) increases bone formation and prevents bone loss in hindlimb-unloaded (HLU) rats. However, the mechanisms of action of PTH are incompletely known. To explore possible interactions between weight bearing and PTH, we treated 6-mo-old weight-bearing and HLU rats with a human therapeutic dose (1 mu g center dot kg(-1)center dot day(-1)) of human PTH (1-34) (hPTH). Cortical and cancellous bone formation was measured in tibia at the diaphysis proximal to the tibia-fibula synostosis and at the proximal metaphysis, respectively. Two weeks of hindlimb unloading resulted in a dramatic decrease in the rate of bone formation at both skeletal sites, which was prevented by PTH treatment at the cancellous site only. In contrast, PTH treatment increased cortical as well as cancellous bone formation in weight-bearing rats. Two-way ANOVA revealed that hPTH and HLU had independent and opposite effects on all histomorphometric indexes of bone formation [mineral apposition rate (MAR), double-labeled perimeter (dLPm), and bone formation rate (BFR)] at both skeletal sites. The bone anabolic effects of weight bearing and hPTH on dLPm and BFR at the cortical site were additive, as were the effects on MAR at the cancellous site. In contrast, weight bearing and hPTH resulted in synergistic increases in cortical bone MAR and cancellous bone dLPm and BFR. We conclude that weight bearing and PTH act cooperatively to increase bone formation by resulting in site-specific additive and synergistic increases in indexes of osteoblast number and activity, suggesting that weight-bearing exercise targeted to osteopenic skeletal sites may improve the efficacy of PTH therapy for osteoporosis. C1 Oregon State Univ, Dept Nutr & Exercise Sci, Corvallis, OR 97333 USA. Mayo Clin & Mayo Fdn, Coll Med, Dept Orthoped, Rochester, MN 55905 USA. NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Turner, RT (reprint author), Oregon State Univ, Dept Nutr & Exercise Sci, 107 Milam Hall, Corvallis, OR 97333 USA. EM russell.turner@oregonstate.edu FU NIAMS NIH HHS [AR-48833] NR 33 TC 27 Z9 30 U1 0 U2 2 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 SEP PY 2006 VL 101 IS 3 BP 881 EP 886 DI 10.1152/japplphysiol.01622.2005 PG 6 WC Physiology; Sport Sciences SC Physiology; Sport Sciences GA 078SQ UT WOS:000240124100027 PM 16675609 ER PT J AU Kondo, H Limol, C Searby, ND Almeida, E Loftus, DJ Vercoutere, W Phillips, J Hilton, D Mojarrab, R Globus, RK AF Kondo, H. Limol, C. Searby, N. D. Almeida, E. Loftus, D. J. Vercoutere, W. Phillips, J. Hilton, D. Mojarrab, R. Globus, R. K. TI Radiation and hypergravity both stimulate production of reactive oxygen species by bone marrow cells, and cell growth and differentiation. SO JOURNAL OF BONE AND MINERAL RESEARCH LA English DT Meeting Abstract CT 28th Annual Meeting of the American-Society-for-Bone-and-Mineral-Research CY SEP 15-19, 2006 CL Philadelphia, PA SP Amer Soc Bone & Mineral Res C1 NASA, Ames Res Ctr, Bone & Signaling Lab, Moffett Field, CA 94035 USA. Univ Calif Irvine, Orange, CA 92668 USA. NR 0 TC 0 Z9 0 U1 0 U2 2 PU AMER SOC BONE & MINERAL RES PI WASHINGTON PA 2025 M ST, N W, STE 800, WASHINGTON, DC 20036-3309 USA SN 0884-0431 J9 J BONE MINER RES JI J. Bone Miner. Res. PD SEP PY 2006 VL 21 SU 1 BP S373 EP S373 PG 1 WC Endocrinology & Metabolism SC Endocrinology & Metabolism GA 089FS UT WOS:000240866303112 ER PT J AU Muir, J Evans, H Judex, S Qin, Y Lang, T Rubin, CT AF Muir, J. Evans, H. Judex, S. Qin, Y. Lang, T. Rubin, C. T. TI Extended bed-rest, like spaceflight, causes rapid and significant loss of bone mineral density and postural control. SO JOURNAL OF BONE AND MINERAL RESEARCH LA English DT Meeting Abstract CT 28th Annual Meeting of the American-Society-for-Bone-and-Mineral-Research CY SEP 15-19, 2006 CL Philadelphia, PA SP Amer Soc Bone & Mineral Res C1 SUNY Stony Brook, Stony Brook, NY 11794 USA. NASA, Lyndon B Johnson Space Ctr, Wyle Labs, Houston, TX 77058 USA. Univ Calif San Francisco, San Francisco, CA 94143 USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU AMER SOC BONE & MINERAL RES PI WASHINGTON PA 2025 M ST, N W, STE 800, WASHINGTON, DC 20036-3309 USA SN 0884-0431 J9 J BONE MINER RES JI J. Bone Miner. Res. PD SEP PY 2006 VL 21 SU 1 BP S376 EP S377 PG 2 WC Endocrinology & Metabolism SC Endocrinology & Metabolism GA 089FS UT WOS:000240866303125 ER PT J AU Phillips, JA Hill, EL Aguirre, JI Wronski, TJ Fassler, R Almeida, EAC Globus, RK AF Phillips, J. A. Hill, E. L. Aguirre, J. I. Wronski, T. J. Fassler, R. Almeida, E. A. C. Globus, R. K. TI Role for beta1 integrin in response of cortical bone to disuse. SO JOURNAL OF BONE AND MINERAL RESEARCH LA English DT Meeting Abstract CT 28th Annual Meeting of the American-Society-for-Bone-and-Mineral-Research CY SEP 15-19, 2006 CL Philadelphia, PA SP Amer Soc Bone & Mineral Res C1 NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. Univ Florida, Dept Physiol Sci, Gainesville, FL 32610 USA. Max Planck Inst Biochem, Dept Mol Med, D-82152 Martinsried, Germany. NR 0 TC 0 Z9 0 U1 0 U2 0 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0884-0431 J9 J BONE MINER RES JI J. Bone Miner. Res. PD SEP PY 2006 VL 21 SU 1 BP S48 EP S48 PG 1 WC Endocrinology & Metabolism SC Endocrinology & Metabolism GA 089FS UT WOS:000240866300177 ER PT J AU Qin, Y Xia, Y Lin, W Evans, H Judex, S Rubin, C AF Qin, Y. Xia, Y. Lin, W. Evans, H. Judex, S. Rubin, C. TI Bone quality and quantity assessment in 90-day bed rest using confocal scanning ultrasound system and DEXA measurement. SO JOURNAL OF BONE AND MINERAL RESEARCH LA English DT Meeting Abstract CT 28th Annual Meeting of the American-Society-for-Bone-and-Mineral-Research CY SEP 15-19, 2006 CL Philadelphia, PA SP Amer Soc Bone & Mineral Res C1 NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. SUNY Stony Brook, Stony Brook, NY 11794 USA. NR 0 TC 1 Z9 1 U1 0 U2 0 PU AMER SOC BONE & MINERAL RES PI WASHINGTON PA 2025 M ST, N W, STE 800, WASHINGTON, DC 20036-3309 USA SN 0884-0431 J9 J BONE MINER RES JI J. Bone Miner. Res. PD SEP PY 2006 VL 21 SU 1 BP S359 EP S359 PG 1 WC Endocrinology & Metabolism SC Endocrinology & Metabolism GA 089FS UT WOS:000240866303061 ER PT J AU Kim, MK Lau, WKM Chin, M Kim, KM Sud, YC Walker, GK AF Kim, Maeng-Ki Lau, William K. M. Chin, Mian Kim, Kyu-Myong Sud, Y. C. Walker, Greg K. TI Atmospheric teleconnection over Eurasia induced by aerosol radiative forcing during boreal spring SO JOURNAL OF CLIMATE LA English DT Article ID GENERAL-CIRCULATION MODEL; SCHUBERT SCHEME MCRAS; BLACK CARBON AEROSOLS; ASIAN SUMMER MONSOON; OPTICAL-PROPERTIES; TROPOSPHERIC AEROSOL; CLIMATE RESPONSE; ABSORBING AEROSOLS; HYDROLOGICAL CYCLE; SOLAR-RADIATION AB The direct effects of aerosols on global and regional climate during boreal spring are investigated based on numerical simulations with the NASA Global Modeling and Assimilation Office finite-volume general circulation model (fvGCM) with Microphyics of Clouds with the Relaxed-Arakawa Schubert Scheme (McRAS), using aerosol forcing functions derived from the Goddard Ozone Chemistry Aerosol Radiation and Transport model (GOCART). The authors find that anomalous atmospheric heat sources induced by absorbing aerosols (dust and black carbon) excite a planetary-scale teleconnection pattern in sea level pressure, temperature, and geopotential height spanning North Africa through Eurasia to the North Pacific. Surface cooling due to direct effects of aerosols is found in the vicinity and downstream of the aerosol source regions, that is, South Asia, East Asia, and northern and western Africa. Significant atmospheric heating is found in regions with large loading of dust (over northern Africa and the Middle East) and black carbon (over Southeast Asia). Paradoxically, the most pronounced feature in aerosol-induced surface temperature is an east-west dipole anomaly with strong cooling over the Caspian Sea and warming over central and northeastern Asia, where aerosol concentrations are low. Analyses of circulation anomalies show that the dipole anomaly is a part of an atmospheric teleconnection pattern driven by atmospheric heating anomalies induced by absorbing aerosols in the source regions, but the influence was conveyed globally through barotropic energy dispersion and sustained by feedback processes associated with the regional circulations. The surface temperature signature associated with the aerosol-induced teleconnection bears striking resemblance to the spatial pattern of observed long-term trend in surface temperature over Eurasia. Additionally, the boreal spring wave train pattern is similar to that reported by Fukutomi et al. associated with the boreal summer precipitation seesaw between eastern and western Siberia. The results of this study raise the possibility that global aerosol forcing during boreal spring may play an important role in spawning atmospheric teleconnections that affect regional and global climates. C1 NASA, Goddard Space Flight Ctr, Atmospheres Lab, Atmospher Chem & Dynam Branch, Greenbelt, MD 20771 USA. Kongju Natl Univ, Dept Atmospher Sci, Kong Ju 314701, South Korea. Sci Syst & Applicat Inc, Lanham, MD USA. NASA, Goddard Space Flight Ctr, Atmospheres Lab, Climate & Radiat Branch, Greenbelt, MD 20771 USA. SAIC, Gen Sci Operat, Beltsville, MD USA. RP Lau, WKM (reprint author), NASA, Goddard Space Flight Ctr, Atmospheres Lab, Atmospher Chem & Dynam Branch, Code 613, Greenbelt, MD 20771 USA. EM lau@climate.gsfc.nasa.gov RI Chin, Mian/J-8354-2012; Kim, Kyu-Myong/G-5398-2014; Lau, William /E-1510-2012 OI Lau, William /0000-0002-3587-3691 NR 65 TC 37 Z9 39 U1 0 U2 11 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 0894-8755 EI 1520-0442 J9 J CLIMATE JI J. Clim. PD SEP PY 2006 VL 19 IS 18 BP 4700 EP 4718 DI 10.1175/JCLI3871.1 PG 19 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 090XI UT WOS:000240987000014 ER PT J AU Allard, D Ave, M Busca, N Malkan, MA Olinto, AV Parizot, E Stecker, FW Yamamoto, T AF Allard, D. Ave, M. Busca, N. Malkan, M. A. Olinto, A. V. Parizot, E. Stecker, F. W. Yamamoto, T. TI Cosmogenic neutrinos from the propagation of ultrahigh energy nuclei SO JOURNAL OF COSMOLOGY AND ASTROPARTICLE PHYSICS LA English DT Article DE ultra high energy cosmic rays; ultra high energy photons and neutrinos; inter-galactic medium ID COSMIC-RAYS; TAU-NEUTRINOS; GAMMA-RAYS; DEEP-FIELD; SPECTRUM; GALAXIES; UNIVERSE; SIMULATIONS; DETECTOR; PHOTONS AB We calculate the flux of neutrinos generated by the propagation of ultrahigh energy nuclei over cosmological distances. The propagation takes into account the interactions with cosmic background radiations including the CMB and the most recent estimates of higher energy (infrared, optical, and ultraviolet) backgrounds. We assume that the composition of ultrahigh energy cosmic rays (UHECRs) at the source is the same as the one observed at low energies. This assumption fits the present data well at the highest energies. We compare the cosmogenic neutrino flux from mixed composition sources to that from pure proton sources. We find that the neutrino flux in the mixed composition case has a high energy peak, mainly due to photopion production off CMB photons, of similar shape and amplitude to those in the proton case. At low energies both composition cases have significant neutrino flux with a peak around 10(14.5) eV due to the higher energy backgrounds. The mixed composition case induces a higher flux of neutrinos at energies below 10(13) eV due to the neutron decay component that extends down to low energies. Detection of diffuse neutrino fluxes at ultrahigh energies can strongly constrain the source distribution of UHECRs whereas fluxes at lower energies could be used to constrain confinement of VHE and UHE cosmic rays if combined with composition analysis from cosmic ray experiments. C1 Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA. Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA. Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA. Univ Chicago, Dept Phys, Chicago, IL 60637 USA. Univ Calif Los Angeles, Los Angeles, CA 90095 USA. Univ Paris 11, Inst Phys Nucl, IN2P3 CNRS, F-91406 Orsay, France. Univ Calif Los Angeles, NASA, Goddard Space Flight Ctr, Dept Phys & Astron, Los Angeles, CA 90024 USA. RP Allard, D (reprint author), Univ Chicago, Kavli Inst Cosmol Phys, 5640 S Ellis, Chicago, IL 60637 USA. EM denis@oddjob.uchicago.edu; ave@cfcp.uchicago.edu; ngb@uchicago.edu; malkan@astro.ucla.edu; olinto@oddjob.uchicago.edu; parizot@ipno.in2p3.fr; Floyd.W.Stecker@nasa.gov; yamamoto@oddjob.uchicago.edu RI Stecker, Floyd/D-3169-2012 NR 65 TC 34 Z9 35 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 1475-7516 J9 J COSMOL ASTROPART P JI J. Cosmol. Astropart. Phys. PD SEP PY 2006 IS 9 AR 005 DI 10.1088/1475-7516/2006/09/005 PG 22 WC Astronomy & Astrophysics; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA 111KG UT WOS:000242449600005 ER PT J AU Dukhan, N Picon-Feliciano, R Alvarez-Hernandez, AR AF Dukhan, Nihad Picon-Feliciano, Ruben Alvarez-Hernandez, Angel R. TI Air flow through compressed and uncompressed aluminum foam: Measurements and correlations SO JOURNAL OF FLUIDS ENGINEERING-TRANSACTIONS OF THE ASME LA English DT Article DE pressure drop; permeability; metal foam; porous media ID METAL FOAMS; POROUS-MEDIA; HEAT-EXCHANGERS; PRESSURE-DROP; PERMEABILITY AB Wind-tunnel steady-state unidirectional pressure-drop measurements for airflow through nine compressed and uncompressed isotropic open-cell aluminum,foam samples, having different porosities and pore densities, were undertaken. The compressed foam produced significantly higher pressure drop, which increased with increasing Darcian velocity following the quadratic Forchheimer equation. The permeability and the inertia coefficient data for the compressed foam showed less scatter compared to those for the uncompressed foam. Both were correlated using an Ergun-like equation, with the correlation being better for the permeability. The permeability, correlation predicted the results of some previous studies very well. The friction factor correlated well with the Reynolds number. C1 Univ Detroit Mercy, Dept Mech Engn, Detroit, MI 48221 USA. Univ Puerto Rico, Dept Mech Engn, Mayaguez, PR 00681 USA. NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. RP Dukhan, N (reprint author), Univ Detroit Mercy, Dept Mech Engn, Detroit, MI 48221 USA. EM nihad.dukhan@udmercy.edu; ruben-picon@hotmail.com; angel-alvarez-hernandez@yahoo.com NR 33 TC 20 Z9 24 U1 1 U2 6 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 SEP PY 2006 VL 128 IS 5 BP 1004 EP 1012 DI 10.1115/1.2236132 PG 9 WC Engineering, Mechanical SC Engineering GA 088JL UT WOS:000240807900013 ER PT J AU Frolking, S Milliman, T McDonald, K Kimball, J Zhao, MS Fahnestock, M AF Frolking, Steve Milliman, Tom McDonald, Kyle Kimball, John Zhao, Maosheng Fahnestock, Mark TI Evaluation of the SeaWinds scatterometer for regional monitoring of vegetation phenology SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID NET PRIMARY PRODUCTION; ERS-SCATTEROMETER; SOIL-MOISTURE; MODIS DATA; WALNUT ORCHARD; TAIGA FORESTS; BACKSCATTER; MODEL; VARIABILITY; PATTERNS AB [ 1] Phenology, or the seasonality of recurring biological events such as vegetation canopy development and senescence, is a primary constraint on global carbon, water and energy cycles. We analyzed multiseason Ku-band radar backscatter measurements from the SeaWinds-on-QuikSCAT scatterometer to determine canopy phenology and growing season vegetation dynamics from 2000 to 2002 at 27 sites representing major global land cover classes and regionally across most of North America. We compared these results with similar information derived from the MODIS leaf area index (LAI) data product (MOD-15A2). In site-level linear regression analysis, the correspondence between radar backscatter and LAI was significant ( p < 0.05) at most but not all sites and was generally higher (R-2 > 0.5) for sites with relatively low LAI or where the seasonal range in LAI was large (e.g., > 3 m(2) m(-2)). The SeaWinds instrument also detected generally earlier onset of vegetation canopy growth in spring than the optical/near-infrared (NIR) based LAI measurements from MODIS, though the timing of canopy senescence and the end of the growing season were more similar. Over North America, the correlation between the two time series was stratified largely by land cover class, with higher correlations (R similar to 0.7 - 0.9) for most cropland, deciduous broadleaf forest, crop/natural vegetation mosaic land cover, and some grassland. Lower correlations were observed for open shrubland and evergreen needleleaf forest. Overall, the results indicate that SeaWinds backscatter is sensitive to growing season canopy dynamics across a range of broadleaf vegetation types and provides a quantitative view that is independent of optical/NIR remote sensing instruments. C1 Univ New Hampshire, Inst Study Earth Oceans & Space, Durham, NH 03824 USA. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. Univ Montana, Flathead Lake Biol Stn, Div Biol Sci, Missoula, MT 59812 USA. Univ Montana, Numer Terradynam Simulat Grp, Missoula, MT 59812 USA. RP Frolking, S (reprint author), Univ New Hampshire, Inst Study Earth Oceans & Space, 39 Coll Rd, Durham, NH 03824 USA. EM steve.frolking@unh.edu RI Zhao, Maosheng/G-5706-2010; Fahnestock, Mark/N-2678-2013; OI Milliman, Thomas/0000-0001-6234-8967 NR 59 TC 24 Z9 24 U1 0 U2 16 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X EI 2169-8996 J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD SEP 1 PY 2006 VL 111 IS D17 AR D17302 DI 10.1029/2005JD006588 PG 14 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 081RA UT WOS:000240333500001 ER PT J AU Kato, S Hinkelman, LM Cheng, AN AF Kato, Seiji Hinkelman, Laura M. Cheng, Anning TI Estimate of satellite-derived cloud optical thickness and effective radius errors and their effect on computed domain-averaged irradiances SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID ATMOSPHERE RADIATIVE FLUXES; BOUNDARY-LAYER CLOUDS; ENERGY SYSTEM CERES; ISCCP DATA SETS; INDEPENDENT PIXEL; TOP; RESOLUTION; SURFACE; ALBEDO; UNCERTAINTIES AB [ 1] The process of retrieving cloud optical thickness and effective radius from radiances measured by satellite instruments is simulated to determine the error in both the retrieved properties and in the irradiances computed with them. The radiances at 0.64 mu m and 3.7 mu m are computed for three cloud fields ( stratus, stratocumulus, and cumulus) generated by large eddy simulation models. When overcast pixels are assumed and the horizontal flux is neglected in the retrieval process, the error in the domain-averaged retrieved optical thickness from nadir is 1% to - 32% ( 1% to - 27%) and the error in the retrieved effective radius is 0% to 67% ( 0% to 63%) for the solar zenith angle of 30 degrees (50 degrees). Using the radiance averaged over a 1 km size pixel also introduces error in the optical thickness because of the nonlinear relation between the reflected radiance and optical thickness. Both optical thickness and effective radius errors increase with increasing horizontal inhomogeneity. When the 0.64 mm albedo is computed with the independent column approximation using retrieved properties from nadir ( oblique) view for a solar zenith angle of 50 degrees, the error is - 0.3% to 14% ( - 5% to - 30%) relative to the albedo from 3-D radiative transfer computations with the true cloud properties. The albedo error occurs even though the radiance at one angle is forced to agree because a plane parallel cloud with a single value of optical thickness and effective radius cannot consistently match the radiance angular distribution. In addition, the error in the retrieved cloud properties contributes to the albedo error. When albedos computed with cloud properties derived from nadir and oblique views are averaged, the albedo error can partially cancel. The absolute error in the narrowband 0.64 mu m (3.7 mu m) albedo averaged over a 1 degrees x 1 degrees domain is less than 1.5% (0.6%), 5.0% (4.1%), and 7.1% (11%) in order of increasing inhomogeneity, when albedos computed with cloud properties derived from viewing zenith angles between 0 degrees and 60 degrees are averaged and when the solar zenith angle is between 10 degrees and 50 degrees. When the solar zenith angle is 70 degrees, the error increases to up to + 24% (+ 37%) for all three scenes. C1 Hampton Univ, Ctr Atmospher Sci, Hampton, VA 23668 USA. Natl Inst Aerosp, Hampton, VA USA. RP Kato, S (reprint author), NASA, Langley Res Ctr, Mail Stop 420, Hampton, VA 23681 USA. EM s.kato@larc.nasa.gov; laura@nianet.org; anningc@yahoo.com RI Hinkelman, Laura/L-8964-2016 OI Hinkelman, Laura/0000-0001-6477-9648 NR 35 TC 28 Z9 28 U1 0 U2 4 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD SEP 1 PY 2006 VL 111 IS D17 AR D17201 DI 10.1029/2005JD006668 PG 16 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 081RA UT WOS:000240333500002 ER PT J AU Cohen, EA Goodridge, DM Kawaguchi, K Fink, EH Setzer, KD AF Cohen, E. A. Goodridge, D. M. Kawaguchi, K. Fink, E. H. Setzer, K. D. TI The rotational spectrum of BiO radical in its X-1 (2)Pi(1/2) and X-2 (2)Pi(3/2) states SO JOURNAL OF MOLECULAR SPECTROSCOPY LA English DT Article DE BiO radical; rotational spectra; hyperfine parameters; relativistic effects ID FINE-STRUCTURE TRANSITION; MICROWAVE SPECTROSCOPY; HYPERFINE STRUCTURE; ELECTRONIC STATES; HIGH-RESOLUTION; AB-INITIO; CONFIGURATION; FREQUENCIES; PARAMETERS; CONSTANTS AB Rotational spectra have been observed for BiO produced in a DC discharge through a low pressure mixture Of O-2, Ar, and Bi vapor. Because of the highly non-thermal distribution of states, it has been possible to observe spectra arising from the X-1(2) Pi(1/2) level up to v = 9 and for the X-2 (2)Pi(3/2) level up to v = 5 near 10538 cm(-1). Precise rotational and hyperfine parameters have been determined for the observed states. By using available near infrared (NIR) data in a merged fit, the 0-0 and 1-1 fine structure intervals have been more precisely determined. Although the quality of the fit is very good, the interpretation of the hyperfine constants is complicated by relativistic effects and the interaction of the X-2 state with A(1) (4)Pi(3/2) state. The magnetic and quadrupole coupling constants will be compared with those of the Bi atom and related molecules. (c) 2006 Elsevier Inc. All rights reserved. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. Conexio Genom, Applecross, WA 6953, Australia. Okayama Univ, Dept Chem, Okayama, Japan. Berg Univ Gesamthsch Wuppertal, Fachbereich Phys Chem, D-42097 Wuppertal, Germany. RP Cohen, EA (reprint author), 4636 El Camino Corto, La Canada Flintridge 91011, CA USA. EM eajscohen@earthlink.net RI Kawaguchi, Kentarou/B-1758-2011 OI Kawaguchi, Kentarou/0000-0003-1067-1839 NR 32 TC 4 Z9 5 U1 1 U2 1 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 SEP PY 2006 VL 239 IS 1 BP 16 EP 23 DI 10.1016/j.jms.2006.05.011 PG 8 WC Physics, Atomic, Molecular & Chemical; Spectroscopy SC Physics; Spectroscopy GA 081ER UT WOS:000240300500003 ER PT J AU Cabanes, C Huck, T De Verdiere, AC AF Cabanes, Cecile Huck, Thierry De Verdiere, Alain Colin TI Contributions of wind forcing and surface heating to interannual sea level variations in the Atlantic Ocean SO JOURNAL OF PHYSICAL OCEANOGRAPHY LA English DT Article ID SUBPOLAR NORTH-ATLANTIC; ROSSBY WAVES; PACIFIC-OCEAN; SOUTH-PACIFIC; VARIABILITY; TOPEX/POSEIDON; CIRCULATION; HEIGHT; FREQUENCIES; ALTIMETER AB Interannual sea surface height variations in the Atlantic Ocean are examined from 10 years of high-precision altimeter data in light of simple mechanisms that describe the ocean response to atmospheric forcing: 1) local steric changes due to surface buoyancy forcing and a local response to wind stress via Ekman pumping and 2) baroclinic and barotropic oceanic adjustment via propagating Rossby waves and quasi-steady Sverdrup balance, respectively. The relevance of these simple mechanisms in explaining interannual sea level variability in the whole Atlantic Ocean is investigated. It is shown that, in various regions, a large part of the interannual sea level variability is related to local response to heat flux changes (more than 50% in the eastern North Atlantic). Except in a few places, a local response to wind stress forcing is less successful in explaining sea surface height observations. In this case, it is necessary to consider large-scale oceanic adjustments: the first baroclinic mode forced by wind stress explains about 70% of interannual sea level variations in the latitude band 18 degrees - 20 degrees N. A quasi-steady barotropic Sverdrup response is observed between 40 degrees and 50 degrees N. C1 Lab Phys Ocean, Brest, France. RP Cabanes, C (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr,M-S 300-323, Pasadena, CA 91109 USA. EM ccabanes@pacific.jpl.nasa.gov RI Huck, Thierry/L-5549-2015 OI Huck, Thierry/0000-0002-2885-5153 NR 30 TC 35 Z9 42 U1 0 U2 2 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 0022-3670 J9 J PHYS OCEANOGR JI J. Phys. Oceanogr. PD SEP PY 2006 VL 36 IS 9 BP 1739 EP 1750 DI 10.1175/JPO2935.1 PG 12 WC Oceanography SC Oceanography GA 091PO UT WOS:000241041000004 ER PT J AU Rock, BS Blandino, JJ Anderson, KR Polk, JE AF St. Rock, B. Blandino, J. J. Anderson, K. R. Polk, J. E. TI Thermal analysis of a lithium vaporizer for a high-power magnetoplasmadynamic thruster SO JOURNAL OF PROPULSION AND POWER LA English DT Article; Proceedings Paper CT AIAA/ASME/SAE/ASEE 41st Joint Propulsion Conference CY JUL 10-13, 2005 CL Tucson, AZ SP AIAA, ASME, SAE, ASEE ID HEAT-TRANSFER AB The lithium vaporizer for a high-power magnetoplasmadynamic thruster is modeled using a 1-D, thermal-resistive network. We use this model to calculate the required vaporizer length and power as a function of mass How rate, channel geometry, and material properties. After comparing results predicted by this model with preheat power data for a 200 kW thruster, we investigate performance over a parameter space of interest for the Advanced Lithium-Fed Appled-Field Lorentz Force Accelerator thruster. Heater power sensitivity to cathode tube emissivity, mass flow rate, and vapor superheat are presented. The cold-start heater power for 80 mg/s is found to range from 3.38 to 3.60 kW, corresponding to a vaporizer (axial) length of 18 to 26 cm. The strongest drivers of vaporizer performance are cathode tube emissivity and the conduction heat flow path through the mounting flange. Also, for the baseline case, it is shown that increasing the vapor superheat from 100 to 300 K has the effect of lowering the vaporizer thermal efficiency from 57 to 49%. Finally, the network model results are used to provide boundary conditions for a finite-element thermal model of the cathode assembly. This model is used to calculate a higher resolution temperature distribution throughout the cathode assembly. C1 Worcester Polytech Inst, Dept Mech Engn, Worcester, MA 01609 USA. NASA, Jet Prop Lab, Pasadena, CA 91109 USA. RP Rock, BS (reprint author), Worcester Polytech Inst, Dept Mech Engn, Worcester, MA 01609 USA. NR 26 TC 1 Z9 1 U1 0 U2 0 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 SEP-OCT PY 2006 VL 22 IS 5 BP 1098 EP 1110 DI 10.2514/1.19773 PG 13 WC Engineering, Aerospace SC Engineering GA 086JX UT WOS:000240670700019 ER PT J AU Toth, RA Brown, LR Smith, MAH Devi, VM Benner, DC Dulick, M AF Toth, RA Brown, LR Smith, MAH Devi, VM Benner, DC Dulick, M TI Air-broadening of H2O as a function of temperature: 696-2163 cm(-1) SO JOURNAL OF QUANTITATIVE SPECTROSCOPY & RADIATIVE TRANSFER LA English DT Article DE water; air-broadened widths; temperature dependence ID WATER-VAPOR; PARAMETERS; LINES; SHIFTS AB The temperature dependence of air-broadened half-widths are reported for some 500 transitions in the (000)-(000) and (010)-(000) bands of (H2O)-O-16 using gas sample temperatures ranging from 241 to 388 K. These observations were obtained from infrared laboratory spectra recorded at 0.006-0.011 cm(-1) resolution with the McMath-Pierce Fourier transform spectrometer located at Kitt Peak. The experimental values of the temperature dependence exponents, eta, were grouped into eight subsets and fitted to empirical functions in a semi-global procedure. Overall, the values of eta were found to decrease with increasing rotational quantum number J. The number of measurements (over 2200) and transitions (586) involved exceeds by a large margin that of any other comparable reported study. (C) 2005 Elsevier Ltd. All rights reserved. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. NASA, Langley Res Ctr, Sci Directorate, Hampton, VA 23681 USA. Coll William & Mary, Williamsburg, VA 23187 USA. Natl Solar Observ, Tucson, AZ 85726 USA. RP Toth, RA (reprint author), CALTECH, Jet Prop Lab, MS 183-301,4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM toth@caesar.jpl.nasa.gov NR 12 TC 26 Z9 26 U1 1 U2 1 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0022-4073 J9 J QUANT SPECTROSC RA JI J. Quant. Spectrosc. Radiat. Transf. PD SEP PY 2006 VL 101 IS 2 BP 339 EP 366 DI 10.1016/j.jqsrt.2005.11.022 PG 28 WC Optics; Spectroscopy SC Optics; Spectroscopy GA 057LW UT WOS:000238598300013 ER PT J AU Salas, MD AF Salas, M. D. TI Digital flight: The last CFD aeronautical grand challenge SO JOURNAL OF SCIENTIFIC COMPUTING LA English DT Article DE aircraft stability and control; external aerodynamics; computational fluid dynamics; flight simulation; grid convergence ID NAVIER-STOKES EQUATIONS; TURBULENT FLOWS AB A case is made for a computational fluid dynamics (CFD) effort to predict aircraft flight characteristics, with a focus on stability and control. Problems in predicting stability and control are discussed. The state-of-the-art in CFD, as it relates to aircraft flight predictions, is reviewed. Problems affecting grid convergence studies are analyzed. The computer resources needed to address flight simulation problems are estimated. The status of critical technologies is briefly discussed. C1 NASA, Langley Res Ctr, Hampton, VA 23681 USA. RP Salas, MD (reprint author), NASA, Langley Res Ctr, Mail Stop 499, Hampton, VA 23681 USA. EM m.d.salas@nasa.gov NR 67 TC 13 Z9 23 U1 0 U2 6 PU SPRINGER/PLENUM PUBLISHERS PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0885-7474 J9 J SCI COMPUT JI J. Sci. Comput. PD SEP PY 2006 VL 28 IS 2-3 BP 479 EP 505 DI 10.1007/s10915-006-9087-7 PG 27 WC Mathematics, Applied SC Mathematics GA 078MA UT WOS:000240106000019 ER PT J AU Wright, MJ Milos, FS Tran, P AF Wright, Michael J. Milos, Frank S. Tran, Philippe TI Afterbody aeroheating flight data for planetary probe thermal protection system design SO JOURNAL OF SPACECRAFT AND ROCKETS LA English DT Article ID MARS-PATHFINDER ENTRY; HEAT-TRANSFER; TRANSITION CORRELATIONS; HYPERSONIC WAKES; TEMPERATURE DATA; NEAR-WAKE; ABLATION; FLOW; VEHICLE C1 NASA, Ames Res Ctr, Moffett Field, CA 95050 USA. EADS SPACE Transportat, F-78133 Les Mureaux, France. RP Wright, MJ (reprint author), NASA, Ames Res Ctr, Moffett Field, CA 95050 USA. NR 92 TC 11 Z9 11 U1 2 U2 7 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 SEP-OCT PY 2006 VL 43 IS 5 BP 929 EP 943 DI 10.2514/1.17703 PG 15 WC Engineering, Aerospace SC Engineering GA 101PQ UT WOS:000241753200001 ER PT J AU Desai, PN Schoenenberger, M Cheatwood, FM AF Desai, Prasun N. Schoenenberger, Mark Cheatwood, F. M. TI Mars Exploration Rover six-degree-of-freedom entry trajectory analysis SO JOURNAL OF SPACECRAFT AND ROCKETS LA English DT Article; Proceedings Paper CT AIAA/AAS Astrodynamics Specialist Conference CY AUG 03-07, 2003 CL Big Sky, MT SP Amer Inst Aeronaut & Astronaut, AAS ID SAMPLE RETURN CAPSULE; DISPERSION ANALYSIS AB The Mars Exploration Rover mission delivered the rovers Spirit and Opportunity to the surface of Mars using the same entry, descent, and landing scenario that was developed and successfully implemented by Mars Pathfinder. This investigation describes the premission trajectory analysis that was performed for the hypersonic portion of the Mars Exploration Rover entry up to parachute deployment. In this analysis, a six-degree-of-freedom trajectory simulation of the entry is performed to determine the entry characteristics of the capsules. In addition, a Monte Carlo dispersion analysis is also performed to statistically assess the robustness of the entry design to off-nominal conditions to ensure that all entry requirements are satisfied. The premission results show that the attitude at peak heating and parachute deployment are well within entry limits. In addition, the parachute deployment dynamic pressure and Mach number are also well within the design requirements. C1 NASA, Langley Res Ctr, Explorat Syst Engn Branch, Syst Engn Directorate, Hampton, VA 23681 USA. NASA, Langley Res Ctr, Space Operat Program, Explorat Syst & Space Operat Technol Directorate, Hampton, VA 23681 USA. NASA, Langley Res Ctr, Space Technol Program, Explorat Syst & Space Operat Technol Directorate, Hampton, VA 23681 USA. RP Desai, PN (reprint author), NASA, Langley Res Ctr, Explorat Syst Engn Branch, Syst Engn Directorate, Hampton, VA 23681 USA. EM prasun.n.desai@nasa.gov; m.schoenenberger-1@nasa.gov; f.m.cheatwood@nasa.gov NR 15 TC 20 Z9 22 U1 0 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 SEP-OCT PY 2006 VL 43 IS 5 BP 1019 EP 1025 DI 10.2514/1.6008 PG 7 WC Engineering, Aerospace SC Engineering GA 101PQ UT WOS:000241753200010 ER PT J AU Braun, RD Wright, HS Croom, MA Levine, JS Spencer, DA AF Braun, Robert D. Wright, Henry S. Croom, Mark A. Levine, Joel S. Spencer, David A. TI Design of the ARES Mars airplane and mission architecture SO JOURNAL OF SPACECRAFT AND ROCKETS LA English DT Article AB Significant technology advances have enabled planetary aircraft to be considered as viable science platforms. Such systems fill a unique planetary. science measurement gap, that of regional-scale, near-surface observation, while providing a fresh perspective for potential discovery. Recent efforts have produced mature mission and flight system concepts, ready for flight project implementation. The development of a Mars airplane mission architecture that balances science, implementation risk, and cost is summarized. Airplane mission performance, flight system design, and technology maturation are described. The design, analysis, and testing completed demonstrates the readiness of this science platform for use in a Mars flight project. C1 Georgia Inst Technol, Guggenheim Sch Aerosp Engn, Atlanta, GA 30332 USA. NASA, Langley Res Ctr, Syst Engn Directorate, Hampton, VA 23681 USA. NASA, Langley Res Ctr, Res Technol Directorate, Hampton, VA 23681 USA. NASA, Langley Res Ctr, Sci Directorate, Hampton, VA 23681 USA. CALTECH, Jet Prop Lab, Phoenix Mars Scout Project, Pasadena, CA 91109 USA. RP Braun, RD (reprint author), Georgia Inst Technol, Guggenheim Sch Aerosp Engn, Atlanta, GA 30332 USA. NR 17 TC 9 Z9 10 U1 0 U2 8 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 SEP-OCT PY 2006 VL 43 IS 5 BP 1026 EP 1034 DI 10.2514/1.17956 PG 9 WC Engineering, Aerospace SC Engineering GA 101PQ UT WOS:000241753200011 ER PT J AU Chato, DJ Martin, TA AF Chato, David J. Martin, Timothy A. TI Vented tank resupply experiment: Flight test results SO JOURNAL OF SPACECRAFT AND ROCKETS LA English DT Article AB This paper reports the results of the vented tank resupply experiment which was flown 19 May 1996 as a payload on the space shuttle mission STS 77. The vented tank resupply experiment examines the ability of vane propellant management devices to separate liquid and gas in low gravity. The vented tank resupply experiment used two clear 22.7 liter (0.8 ft(3)) tanks, one spherical and one with a short barrel section. Refrigerant 113 was transferred between the two tanks. The tanks were also periodically vented to space. Tests included the retention of liquid during transfer, liquid-free venting, and recovery of liquid into the propellant management devices after thruster firing. Liquid was retained successfully at the highest flow rate tested (10.33 l/min). Liquid-free vents were achieved for both tanks, although at a higher flow rate (4.51 l/min) for the spherical tank than for the other (1.13 l/min). Recovery from a thruster firing which moved the liquid to the opposite end of the tank from the propellant management devices was achieved in 30 s. C1 NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. Lockheed Martin Space Syst, Denver, CO 80201 USA. RP Chato, DJ (reprint author), NASA, Glenn Res Ctr, Mail Stop 86-2,21000 Brookpk Rd, Cleveland, OH 44135 USA. RI Chato, David/B-2698-2013 OI Chato, David/0000-0003-2990-0646 NR 13 TC 4 Z9 8 U1 0 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 SEP-OCT PY 2006 VL 43 IS 5 BP 1124 EP 1130 DI 10.2514/1.18145 PG 7 WC Engineering, Aerospace SC Engineering GA 101PQ UT WOS:000241753200023 ER PT J AU Galofaro, JT Vayner, BV Degroot, WA Ferguson, DC AF Galofaro, Joel T. Vayner, Boris V. Degroot, Wilhelmus A. Ferguson, Dale C. TI Role of water vapor in solar array arc initiation: Dissociative recombination processes SO JOURNAL OF SPACECRAFT AND ROCKETS LA English DT Article; Proceedings Paper CT AIAA 40th Aerospace Sciences Meeting CY JAN 14-18, 2002 CL RENO, NV SP Amer Inst Aeronaut & Astronaut ID LOW-EARTH-ORBIT; PLASMA INTERACTIONS; VOLTAGE; ENVIRONMENT; DISCHARGES; SPACECRAFT; CURRENTS AB Strong supporting evidence that adsorbed water vapor residing at the triple junction sites on a solar array is a leading contributing factor to arcing onset in conventional silicon photovoltaic arrays immersed in low Earth orbital plasmas is presented. It is suggested that an adsorbed water vapor layer becomes ionized by energetic electrons and that the discharge develops in the area of a triple junction. The fastest process to extinguish the discharge is the dissociative recombination of water molecular ions. Are plasma spectroscopic data throughout the wavelength range 260-680 nm is obtained. The two most intensive silver lines in the UV spectrum (Ag I, 329 and 338 nut), an atomic silver line (Ag I, 358.6 nm), and two lines of singly ionized silver atoms (Ag II, 318.7 and 368.2 nm) are identified. Additionally, atomic line spectra Fe I (415.87 nm) and Ni I (480.7 nm) are found. More importantly, identification of several species that appear to validate a dissociative recombination process involving water vapor is also found. The observations involved are the OH molecular band (302-309 nm) and two intensive atomic lines (H-alpha, 656.3 nm, and H-beta, 486 nm). The following species with molecular bands, CH (432 nm), SiH (387 nm), and SiN (472 nm) are also identified. C1 NASA, John H Glenn Res Ctr Lewis Field, Photovolta & Space Environm Branch, Cleveland, OH 44135 USA. Ohio Aerosp Inst, Cleveland, OH 44192 USA. Silicon Light Inc, Sunnyvale, CA 94087 USA. NASA, George C Marshall Space Flight Ctr, Environm Effects Branch, Huntsville, AL 35812 USA. RP Galofaro, JT (reprint author), NASA, John H Glenn Res Ctr Lewis Field, Photovolta & Space Environm Branch, Cleveland, OH 44135 USA. EM Galofaro@nasa.gov NR 25 TC 0 Z9 0 U1 1 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 SEP-OCT PY 2006 VL 43 IS 5 BP 1131 EP 1135 DI 10.2514/1.21639 PG 5 WC Engineering, Aerospace SC Engineering GA 101PQ UT WOS:000241753200024 ER PT J AU Brady, KM AF Brady, Kevin M. TI True women and westward expansion. SO JOURNAL OF THE EARLY REPUBLIC LA English DT Book Review C1 Texas Christian Univ, Ft Worth, TX 76129 USA. NASA, Lyndon B Johnson Space Ctr, Univ Space Res Assoc, Houston, TX 77058 USA. RP Brady, KM (reprint author), Texas Christian Univ, Ft Worth, TX 76129 USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU SOC HISTORIANS EARLY AMERICAN REPUBLIC PI W LAFAYETTE PA PURDUE UNIV, 1358 UNIV HALL, W LAFAYETTE, IN 47907-1358 USA SN 0275-1275 J9 J EARLY REPUBL JI J. Early Repub. PD FAL PY 2006 VL 26 IS 3 BP 483 EP 487 DI 10.1353/jer.2006.0044 PG 5 WC History SC History GA 080TY UT WOS:000240272600008 ER PT J AU Brady, KM AF Brady, Kevin M. TI Changing national identities at the frontier. Texas and New Mexico, 1800-1850. SO JOURNAL OF THE EARLY REPUBLIC LA English DT Book Review C1 Texas Christian Univ, Ft Worth, TX 76129 USA. NASA, Lyndon B Johnson Space Ctr, Univ Space Res Assoc, Houston, TX 77058 USA. RP Brady, KM (reprint author), Texas Christian Univ, Ft Worth, TX 76129 USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU SOC HISTORIANS EARLY AMERICAN REPUBLIC PI W LAFAYETTE PA PURDUE UNIV, 1358 UNIV HALL, W LAFAYETTE, IN 47907-1358 USA SN 0275-1275 J9 J EARLY REPUBL JI J. Early Repub. PD FAL PY 2006 VL 26 IS 3 BP 483 EP 487 DI 10.1353/jer.2006.0044 PG 5 WC History SC History GA 080TY UT WOS:000240272600009 ER PT J AU Yamakov, V Saether, E Phillips, DR Glaessgen, EH AF Yamakov, V. Saether, E. Phillips, D. R. Glaessgen, E. H. TI Molecular-dynamics simulation-based cohesive zone representation of intergranular fracture processes in aluminum SO JOURNAL OF THE MECHANICS AND PHYSICS OF SOLIDS LA English DT Article DE crack-tip plasticity; cohesive zone model; grain boundary decohesion; intergranular fracture; molecular-dynamics simulation ID CRACK-GROWTH RESISTANCE; TILT GRAIN-BOUNDARIES; ATOMISTIC SIMULATIONS; NANOCRYSTALLINE AL; DEFORMATION; PROPAGATION; MODEL; DISLOCATION; BEHAVIOR; METALS AB A traction-displacement relationship that may be embedded into a cohesive zone model for microscale problems of intergranular fracture is extracted from atomistic molecular-dynamics (MD) simulations. An MD model for crack propagation under steady-state conditions is developed to analyze intergranular fracture along a flat Sigma 99 [I 10] symmetric tilt grain boundary in aluminum. Under hydrostatic tensile load. the simulation reveals asymmetric crack propagation in the two opposite directions along the grain boundary. In one direction, the crack propagates in a brittle manner by cleavage with very little or no dislocation emission, and in the other direction, the propagation is ductile through the mechanism of deformation twinning. This behavior is consistent with the Rice criterion for cleavage vs. dislocation blunting transition at the crack tip. The preference for twinning to dislocation slip is in agreement with the predictions of the Tadmor and Hai criterion. A comparison with finite element calculations shows that while the stress field around the brittle crack tip follows the expected elastic solution for the given boundary conditions of the model, the stress field around the twinning crack tip has a strong plastic contribution. Through the definition of a Cohesive-Zone-Volume-Element-an atomistic analog to a continuum cohesive zone model element-the results from the MD simulation are recast to obtain an average continuum traction-displacement relationship to represent cohesive zone interaction along a characteristic length of the grain boundary interface for the cases of ductile and brittle decohesion. (c) 2006 Elsevier Ltd. All rights reserved. C1 Natl Inst Aerosp, Hampton, VA 23666 USA. NASA, Langley Res Ctr, Hampton, VA 23681 USA. Lockheed Martin Space Operat, Hampton, VA 23681 USA. RP Yamakov, V (reprint author), Natl Inst Aerosp, Hampton, VA 23666 USA. EM yamakov@nianet.org NR 51 TC 95 Z9 100 U1 6 U2 50 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0022-5096 J9 J MECH PHYS SOLIDS JI J. Mech. Phys. Solids PD SEP PY 2006 VL 54 IS 9 BP 1899 EP 1928 DI 10.1016/j.jmps.2006.03.004 PG 30 WC Materials Science, Multidisciplinary; Mechanics; Physics, Condensed Matter SC Materials Science; Mechanics; Physics GA 065BJ UT WOS:000239134100006 ER PT J AU Kumar, SV Doby, TA Baugh, JW Brill, ED Ranjithan, SR AF Kumar, Sujay V. Doby, Troy A. Baugh, John W., Jr. Brill, E. Downey Ranjithan, S. Ranji TI Optimal design of redundant water distribution networks using a cluster of workstations SO JOURNAL OF WATER RESOURCES PLANNING AND MANAGEMENT-ASCE LA English DT Article DE algorithms; water distribution systems; computation; optimization models ID DISTRIBUTION-SYSTEMS; GENETIC ALGORITHMS; OPTIMIZATION; RELIABILITY AB A genetic algorithm (GA)-based method for the least-cost design of looped pipe networks for various levels of redundancy is presented in this paper. Redundancy constraints are introduced in the optimization model by considering the number of pipes assumed to be out of service at any one time. Using this approach, trade-off relationships between cost and redundancy are developed. The GA-based approach is computationally intensive, and implementations on a custom fault-tolerant distributed computing framework, called Vitri, are used to satisfy the computational requirements. The design methodology is applied to two water distribution networks of different sizes, and a comparison of the performance of the distributed GAs for the design problems is also presented. We conclude that a GA-based approach to obtaining cost-effective, redundant solutions for the least-cost design of looped pipe networks can be effectively used on a heterogeneous network of nondedicated workstations. C1 NASA, Goddard Space Flight Ctr, Hydrol Sci Branch, Greenbelt, MD 20771 USA. US EPA, NRMRL, Sustainable Technol Div, Syst Anal Branch, Cincinnati, OH 45268 USA. N Carolina State Univ, Raleigh, NC 27695 USA. RP Kumar, SV (reprint author), NASA, Goddard Space Flight Ctr, Hydrol Sci Branch, Greenbelt, MD 20771 USA. EM sujay@hsb.gsfc.nasa.gov; doby.troy@epamail.epa.gov; jwb@ncsu.edu; brill@ncsu.edu; ranji@ncsu.edu RI Kumar, Sujay/B-8142-2015 NR 30 TC 5 Z9 5 U1 0 U2 1 PU ASCE-AMER SOC CIVIL ENGINEERS PI RESTON PA 1801 ALEXANDER BELL DR, RESTON, VA 20191-4400 USA SN 0733-9496 J9 J WATER RES PL-ASCE JI J. Water Resour. Plan. Manage.-ASCE PD SEP-OCT PY 2006 VL 132 IS 5 BP 374 EP 384 DI 10.1061/(ASCE)0733-9496(2006)132:5(374) PG 11 WC Engineering, Civil; Water Resources SC Engineering; Water Resources GA 081DP UT WOS:000240297700007 ER PT J AU Ju, SJ Harvey, HR Gomez-Gutierrez, J Peterson, WT AF Ju, Se-Jong Harvey, H. Rodger Gomez-Gutierrez, Jaime Peterson, William T. TI The role of lipids during embryonic development of the euphausiids Euphausia pacifica and Thysanoessa spinifera SO LIMNOLOGY AND OCEANOGRAPHY LA English DT Article ID ANTARCTIC KRILL; SINKING RATES; FATTY-ACID; SUPERBA; EGGS; CRYSTALLOROPHIAS; DENSITY; PRESSURE; OCEAN AB To understand the role of lipids during early embryogenesis, major lipid classes together with individual fatty-acid and sterol composition were determined in embryos from multiple developmental stages of the euphausiids Euphausia pacifica and Thysanoessa spinifera. Average lipid content in embryos of E. pacifica and T. spinifera from the earliest stage (multicell) were 4.45 and 3.69 mu g embryo(-1), respectively. During development, the lipid content decreased at similar rates in the embryos of both species. In contrast to many crustacean eggs, phospholipids were the dominant lipid class in all embryonic stages, with decreasing concentrations seen during development. Individual fatty acids and sterols showed selective utilization during early developmental stages. The dominant fatty acids were 16:0 and 16:1 omega 7 and 20:5 omega 3, with most polyunsaturated fatty acids preferentially metabolized throughout early stages. An exception was 22:6 omega 3, which remained near constant through all stages. Cholesterol was the dominant sterol (> 82% of total sterols) in embryos, with only minor changes during development. The appearance of algal sterols and fatty alcohols, including phytol, in T. spinifera embryos suggests that considerable amounts of algal lipids are directly allocated to eggs during vitellogenesis. Despite the substantial changes in lipid amount and composition during embryo development, the presence of phospholipids as the dominate lipid store acts to moderate changes in egg-sinking rate for both species until the late (early and late limb-bud) stages of development. C1 Univ Maryland, Ctr Environm Sci, Chesapeake Biol Lab, Solomons, MD 20688 USA. Ctr Interdisciplinario Ciencias Marinas, Dept Plancton & Ecol Marina, La Paz, Baja California, Mexico. Oregon State Univ, Hatfield Marine Sci Ctr, Natl Marine Fisheries Serv, Newport, OR 97365 USA. RP Ju, SJ (reprint author), Univ Maryland, Ctr Environm Sci, Chesapeake Biol Lab, Solomons, MD 20688 USA. EM sejongju@gmail.com RI Ju, Se-Jong/A-9029-2009 NR 40 TC 4 Z9 4 U1 1 U2 8 PU AMER SOC LIMNOLOGY OCEANOGRAPHY PI WACO PA 5400 BOSQUE BLVD, STE 680, WACO, TX 76710-4446 USA SN 0024-3590 J9 LIMNOL OCEANOGR JI Limnol. Oceanogr. PD SEP PY 2006 VL 51 IS 5 BP 2398 EP 2408 PG 11 WC Limnology; Oceanography SC Marine & Freshwater Biology; Oceanography GA 086LC UT WOS:000240673800042 ER PT J AU Moisan, TA Ellisman, MH Buitenhuys, CW Sosinsky, GE AF Moisan, Tiffany A. Ellisman, Mark H. Buitenhuys, Casey W. Sosinsky, Gina E. TI Differences in chloroplast ultrastructure of Phaeocystis antarctica in low and high light SO MARINE BIOLOGY LA English DT Article ID CELL-CENTERED DATABASE; RAT-LIVER MITOCHONDRIA; ELECTRON TOMOGRAPHY; ULTRAVIOLET-RADIATION; PHOTOSYNTHESIS; PHYTOPLANKTON; DIATOMS; SEA AB Phaeocystis antarctica Karsten exhibits optical changes in pigment packaging during acclimation to drastically different light levels. Here, the three-dimensional morphological rearrangements are shown for two light conditions mimicking limiting and saturating conditions for photosynthesis. Cultures of P. antarctica were grown semi-continuously under light-limiting conditions for growth (14 mu mol quanta m(-2) s(-1)) and a light-saturating condition (259 mu mol quanta m(-2) s(-1)) for growth. Increased numbers of thylakoids were observed under the low light treatment. In contrast, there were less amounts of thylakoid stacking in each chloroplast under the high light treatment. Electron microscopic tomographic reconstructions illustrate the complexity of the chloroplast organelle where the thylakoids 'interact' with the pyrenoid and the chloroplast membrane. Highly complex characteristics, such as bi- and tri-furcations in the thylakoid stacks, were continuous throughout the chloroplast. Other organelles, such as the Golgi apparatus and dense vesicles that may potentially affect cellular scattering and absorption were also observed in both high and low light. These three dimensional thylakoid arrangements have profound implications for cellular photophysiology. They represent a new view of algal chloroplast structure, and provide a starting point for more accurate optical modeling studies. C1 NASA, Goddard Space Flight Ctr, Hydrospher & Biospher Sci Lab, Wallops Isl, VA 23337 USA. Univ Calif San Diego, Natl Ctr Microscopy & Imaging Res, Dept Neurosci, La Jolla, CA 92093 USA. Univ Calif San Diego, Ctr Res Biol Syst, La Jolla, CA 92093 USA. RP Moisan, TA (reprint author), NASA, Goddard Space Flight Ctr, Hydrospher & Biospher Sci Lab, Wallops Isl, VA 23337 USA. EM tmoisan@osb.wff.nasa.gov NR 36 TC 9 Z9 9 U1 3 U2 10 PU SPRINGER PI NEW YORK PA 233 SPRING STREET, NEW YORK, NY 10013 USA SN 0025-3162 J9 MAR BIOL JI Mar. Biol. PD SEP PY 2006 VL 149 IS 6 BP 1281 EP 1290 DI 10.1007/s00227-006-0321-5 PG 10 WC Marine & Freshwater Biology SC Marine & Freshwater Biology GA 092QN UT WOS:000241112500001 ER PT J AU Zug, GR Chaloupka, M Balazs, GH AF Zug, George R. Chaloupka, Milani Balazs, George H. TI Age and growth in olive ridley seaturtles (Lepidochelys olivacea) from the north-central Pacific: a skeletochronological analysis SO MARINE ECOLOGY-AN EVOLUTIONARY PERSPECTIVE LA English DT Article DE age; Cheloniidae; Lepidochelys olivacea; growth; humeral skeletal anatomy; non-parametric smoothing; North Pacific Ocean; Reptilia; seaturtle growth modeling; skeletochronology; Testudines ID LOGGERHEAD CARETTA-CARETTA; SEA-TURTLES; SOMATIC GROWTH; KEMPII; VALIDATION; ECOLOGY AB The olive ridley is the most abundant seaturtle species in the world but little is known of the demography of this species. We used skeletochronological data on humerus diameter growth changes to estimate the age of North Pacific olive ridley seaturtles caught incidentally by pelagic longline fisheries operating near Hawaii and from dead turtles washed ashore on the main Hawaiian Islands. Two age estimation methods [ranking, correction factor (CF)] were used and yielded age estimates ranging from 5 to 38 and 7 to 24 years, respectively. Rank age-estimates are highly correlated (r = 0.93) with straight carapace length (SCL), CF age estimates are not (r = 0.62). We consider the CF age-estimates as biologically more plausible because of the disassociation of age and size. Using the CF age-estimates, we then estimate the median age at sexual maturity to be around 13 years old (mean carapace size c. 60 cm SCL) and found that somatic growth was negligible by 15 years of age. The expected age-specific growth rate function derived using numerical differentiation suggests at least one juvenile growth spurt at about 10-12 years of age when maximum age-specific growth rates, c. 5 cm SCL year(-1), are apparent. C1 Natl Museum Nat Hist, Smithsonian Inst, Dept Vertebrate Zool, Washington, DC 20013 USA. Univ Queensland, Ecol Modelling Serv Pty Ltd, St Lucia, Qld, Australia. NOAA, Natl Marine Fisheries Serv, Pacific lsl Fisheries Sci Ctr, Honolulu Lab, Honolulu, HI USA. RP Zug, GR (reprint author), Natl Museum Nat Hist, Smithsonian Inst, Dept Vertebrate Zool, Washington, DC 20013 USA. EM zugg@si.edu NR 33 TC 23 Z9 27 U1 1 U2 11 PU BLACKWELL PUBLISHING PI OXFORD PA 9600 GARSINGTON RD, OXFORD OX4 2DQ, OXON, ENGLAND SN 0173-9565 J9 MAR ECOL-EVOL PERSP JI Mar. Ecol.-Evol. Persp. PD SEP PY 2006 VL 27 IS 3 BP 263 EP 270 DI 10.1111/j.1439-0485.2006.00109.x PG 8 WC Marine & Freshwater Biology SC Marine & Freshwater Biology GA 090PN UT WOS:000240963300008 ER PT J AU Irvine, GV Mann, DH Short, JW AF Irvine, Gall V. Mann, Daniel H. Short, Jeffrey W. TI Persistence of 10-year old Exxon Valdez oil on Gulf of Alaska beaches: The importance of boulder-armoring SO MARINE POLLUTION BULLETIN LA English DT Article DE boulder-armored beaches; Exxon valdez; Gulf of Alaska; oil spill; oil persistence; polycyclic aromatic hydrocarbons (PAH); oil mousse; chemical and physical weathering of oil; petroleum hydrocarbons ID PRINCE-WILLIAM-SOUND; MUSSEL BEDS; SPILL; SEDIMENTS; HYDROCARBONS; TISSUES; GRAVEL AB Oil stranded as a result of the 1989 Exxon Valdez spill has persisted for > 10 years at study sites on Gulf of Alaska shores distant from the spill's origin. These sites were contaminated by "oil mousse", which persists in these settings due to armoring of underlying sediments and their included oil beneath boulders. The boulder-armored beaches that we resampled in 1999 showed continued contamination by subsurface oil, despite their exposure to moderate to high wave energies. Significant declines in surface oil cover occurred at all study sites. In contrast, mousse has persisted under boulders in amounts similar to what was present in 1994 and probably in 1989. Especially striking is the general lack of weathering of this subsurface oil over the last decade. Oil at five of the six armored-beach sites 10 years after the spill is compositionally similar to 11-day old Exxon Valdez oil. Analysis of movements in the boulder-armor that covers the study beaches reveals that only minor shifts have occurred since 1994, suggesting that over the last five, and probably over the last 10 years, boulder-armors have remained largely unmoved at the study sites. These findings emphasize the importance of particular geomorphic parameters in determining stranded oil persistence. Surface armoring, combined with stranding of oil mousse, results in the unexpectedly lengthy persistence of only lightly to moderately weathered oil within otherwise high-energy wave environments. (c) 2006 Elsevier Ltd. All rights reserved. C1 US Geol Survey, Alaska Sci Ctr, Anchorage, AK 99503 USA. Univ Alaska, Inst Arctic Biol, Fairbanks, AK 99775 USA. NOAA, Natl Marine Fisheries Serv, Auke Bay Fisheries Lab, Juneau, AK 99801 USA. RP Irvine, GV (reprint author), US Geol Survey, Alaska Sci Ctr, 1011 E Tudor Rd, Anchorage, AK 99503 USA. EM gail_irvine@usgs.gov NR 33 TC 30 Z9 30 U1 1 U2 12 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0025-326X EI 1879-3363 J9 MAR POLLUT BULL JI Mar. Pollut. Bull. PD SEP PY 2006 VL 52 IS 9 BP 1011 EP 1022 DI 10.1016/j.marpolbul.2006.01.005 PG 12 WC Environmental Sciences; Marine & Freshwater Biology SC Environmental Sciences & Ecology; Marine & Freshwater Biology GA 094PW UT WOS:000241252500013 PM 16524600 ER PT J AU Ciesla, FJ AF Ciesla, Fred J. TI Chondrule collisions in shock waves SO METEORITICS & PLANETARY SCIENCE LA English DT Article ID TURBULENT PROTOPLANETARY NEBULA; COMPOUND CHONDRULES; SOLAR NEBULA; SIZED PARTICLES; HEATING MODEL; CHONDRITES; COALESCENCE; VISCOSITY; IMPACT; LIMITS AB Detailed numerical models have shown that solar nebula shock waves would be able to thermally process chondrules in a way that is consistent with experimental constraints. However, it has recently been argued that the high relative velocities that would be generated between chondrules of different sizes immediately behind the shock front would lead to energetic collisions that would destroy the chondrules as they were processed rather than preserving them for incorporation into meteorite parent bodies. Here the outcome of these collisions is quantitatively explored using a simple analytic expression for the viscous dissipation of collisional energy in a liquid layer. It is shown that molten chondrules can survive collisions at velocities as high as a few hundred meters per second. It is also shown that the thermal evolution of chondrules in a given shock wave varies with chondrule size, which may allow chondrules of different textures to form in a given shock wave. While experiments are needed to further constrain the parameters used in this work, these calculations show that the expected outcomes from collisions behind shock waves are consistent with what is observed in meteorites. C1 NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Ciesla, FJ (reprint author), Carnegie Inst Washington, Dept Terr Magnetism, 5241 Broad Branch Rd NW, Washington, DC 20015 USA. EM ciesla@dtm.ciw.edu NR 48 TC 11 Z9 11 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 SEP PY 2006 VL 41 IS 9 BP 1347 EP 1359 PG 13 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 086GK UT WOS:000240661600006 ER PT J AU Shoemaker, WC Wo, CCJ Lu, K Chien, LC Rhee, P Bayard, D Demetriades, D Jelliffe, RW AF Shoemaker, William C. Wo, Charles C. J. Lu, Kevin Chien, Li- Chien Rhee, Peter Bayard, David Demetriades, Demetrios Jelliffe, Roger W. TI Noninvasive Hemodynamic monitoring for combat casualties SO MILITARY MEDICINE LA English DT Article ID CRITICALLY ILL PATIENTS; EUROPEAN CONSENSUS CONFERENCE; RANDOMIZED CLINICAL-TRIAL; RISK SURGICAL PATIENTS; OXYGEN DELIVERY; PREOPERATIVE OPTIMIZATION; OUTCOME PREDICTION; EMERGENCY PATIENTS; TRAUMA; VALUES AB The aims of this study were to develop and to test a noninvasive hemodynamic monitoring system that could be applied to combat casualties to supplement conventional vital signs, to use an advanced information system to predict outcomes, and to evaluate the relative effectiveness of various therapies with instant feedback information during acute emergency conditions. In a university-run inner city public hospital, we evaluated 1,000 consecutively monitored trauma patients in the initial resuscitation period, beginning shortly after admission to the emergency department. In addition to conventional vital signs, we used noninvasive monitoring devices (cardiac index by bioimpedance with blood pressure and heart rate to measure cardiac function, arterial hemoglobin oxygen saturation by pulse oximetry to reflect changes in pulmonary function, and tissue oxygenation by transcutaneous oxygen tension indexed to fractional inspired oxygen concentration and carbon dioxide tension to evaluate tissue perfusion). The cardiac index, mean arterial pressure, pulse oximetry (arterial hemoglobin oxygen saturation), and transcutaneous oxygen tension/fractional inspired oxygen concentration were significantly higher in survivors, whereas the heart rate and carbon dioxide tension were higher in nonsurvivors. The calculated survival probability was a useful outcome predictor that also served as a measure of severity of illness. The rate of misclassification of survival probability was 13.5% in the series as a whole but only 6% for patients without severe head injuries and brain death. Application of noninvasive hemodynamic monitoring to acute emergency trauma patients in the emergency department is feasible, safe, and inexpensive and provides accurate hemodynamic patterns in continuous, on-line, real-time, graphical displays of the status of cardiac, pulmonary, and tissue perfusion functions. Combined with an information system, this approach provided an early outcome predictor and evaluated, with an objective individualized method, the relative efficacy of alternative therapies for specific patients. C1 Univ So Calif, Los Angeles Cty Med Ctr, Dept Surg, Los Angeles, CA 90033 USA. Univ So Calif, Lab Appl Pharmacokinet, Keck Sch Med, Los Angeles, CA 90089 USA. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Shoemaker, WC (reprint author), Univ So Calif, Los Angeles Cty Med Ctr, Dept Surg, Los Angeles, CA 90033 USA. FU NCRR NIH HHS [RR-11526]; NIGMS NIH HHS [GM-65619] NR 39 TC 7 Z9 8 U1 0 U2 0 PU ASSN MILITARY SURG US PI BETHESDA PA 9320 OLD GEORGETOWN RD, BETHESDA, MD 20814 USA SN 0026-4075 J9 MIL MED JI Milit. Med. PD SEP PY 2006 VL 171 IS 9 BP 813 EP 820 PG 8 WC Medicine, General & Internal SC General & Internal Medicine GA 084LN UT WOS:000240534500002 PM 17036597 ER PT J AU Creighton, T AF Creighton, Teviet TI Astrophysics - An explosion of sound SO NATURE PHYSICS LA English DT News Item AB Astrophysicists have proposed that sound waves could drive some of the largest explosions in the Universe. The emerging field of gravitational-wave astronomy might provide a means to listen in. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Creighton, T (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM teviet@tapir.caltech.edu NR 1 TC 1 Z9 1 U1 0 U2 2 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 1745-2473 J9 NAT PHYS JI Nat. Phys. PD SEP PY 2006 VL 2 IS 9 BP 581 EP 582 DI 10.1038/nphys387 PG 2 WC Physics, Multidisciplinary SC Physics GA 087TT UT WOS:000240766000011 ER PT J AU Schwemmer, GK Rallison, RD Wilkerson, TD Guerra, DV AF Schwemmer, GK Rallison, RD Wilkerson, TD Guerra, DV TI Holographic optical elements as scanning lidar telescopes SO OPTICS AND LASERS IN ENGINEERING LA English DT Article DE scanning lidar; HOE; conical scan; scanning telescope ID WIND MEASUREMENTS; DOPPLER LIDAR; WATER-VAPOR; SYSTEM; COMPENSATION; INSTRUMENT; AIRCRAFT; SENSOR; ZONE; HOES AB We have developed and investigated the use of holographic optical elements (HOEs) and holographic transmission gratings for scanning lidar telescopes. Rotating a flat HOE in its own plane with the focal spot on the rotation axis makes a very simple and compact conical scanning telescope. We developed transmission and reflection HOEs for use at the first three harmonic wavelengths of Nd:YAG lasers. The diffraction efficiency, diffraction angle, focal length, focal spot size and optical losses were measured for several HOEs and holographic gratings, and found to be suitable for use as lidar receiver telescopes, and in many cases could also serve as the final collimating and beam steering optic for the laser transmitter. Two lidar systems based on this technology have been designed, built, and successfully tested in atmospheric science applications. This technology will enable future spaceborne lidar missions by significantly lowering the size, weight, power requirement and cost of a large aperture, narrow field of view scanning telescope. (C) 2005 Elsevier Ltd. All rights reserved. C1 NASA, Goddard Space Flight Ctr, Atmospheres Lab, Greenbelt, MD 20771 USA. Ralcon Inc, Paradise, UT 84328 USA. Utah State Univ, Space Dynam Lab, Logan, UT 84322 USA. St Anselm Coll, Dept Phys, Manchester, NH 03102 USA. RP Schwemmer, GK (reprint author), Sci & Engn Serv Inc, 6992 Columbia Gateway Pkwy,Suite 200, Columbia, MD 21046 USA. EM Geary.K.Schwemmer@nasa.gov; rdr@Ralcon.com; Tom.Wilkerson@sdl.usu.edu; dguerra@anselm.edu NR 38 TC 2 Z9 2 U1 2 U2 5 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 0143-8166 J9 OPT LASER ENG JI Opt. Lasers Eng. PD SEP PY 2006 VL 44 IS 9 BP 881 EP 902 DI 10.1016/j.optlaseng.2005.06.011 PG 22 WC Optics SC Optics GA 049HU UT WOS:000238007900002 ER PT J AU Grudinin, IS Matsko, AB Savchenkov, AA Strekalov, D Ilchenko, VS Maleki, L AF Grudinin, Ivan S. Matsko, Andrey B. Savchenkov, Anatohy A. Strekalov, Dmitry Ilchenko, Vladimir S. Maleki, Lute TI Ultra high Q crystalline microcavities SO OPTICS COMMUNICATIONS LA English DT Article DE whispering gallery modes; microcavity; single mode resonator; diamond turning; cavity QED ID RAYLEIGH-SCATTERING; WAVE-GUIDES; MICROSPHERES; SINGLE; RESONATORS; FILTERS; CAF2; CHIP AB We report on the fabrication technique of ultra high Q optical crystalline whispering gallery mode microresonators and discuss their properties. The technique is suitable for the majority of available optical crystals and for production of resonators with small size. To validate the method, we made CaF2 resonators with Q factors exceeding 4 x 10(8) and a diameter smaller than 100 mu m. A single mode resonator has also been fabricated. Possible utilization of these new resonators in quantum optics is discussed. (c) 2006 Elsevier B.V. All rights reserved. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Grudinin, IS (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM grudinin@caltech.edu RI Matsko, Andrey/A-1272-2007 NR 24 TC 83 Z9 83 U1 4 U2 37 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0030-4018 J9 OPT COMMUN JI Opt. Commun. PD SEP 1 PY 2006 VL 265 IS 1 BP 33 EP 38 DI 10.1016/j.optcom.2006.03.028 PG 6 WC Optics SC Optics GA 080BI UT WOS:000240221400006 ER PT J AU Padula, SL Gumbert, CR Li, W AF Padula, Sharon L. Gumbert, Clyde R. Li, Wu TI Aerospace applications of optimization under uncertainty SO OPTIMIZATION AND ENGINEERING LA English DT Article; Proceedings Paper CT 4th International Symposium on Uncertainty Modeling and Anlysis (ISUMA 03) CY SEP 21-24, 2003 CL Univ Maryland, Baltimore, MD HO Univ Maryland DE Aerospace; Reliability; Probabilistic analysis; Robust optimization AB The Multidisciplinary Optimization (MDO) Branch at NASA Langley Research Center develops new methods and investigates opportunities for applying optimization to aerospace vehicle design. This paper describes MDO Branch experiences with three applications of optimization under uncertainty: (1) improved impact dynamics for airframes, (2) transonic airfoil optimization for low drag, and (3) coupled aerodynamic and structures optimization of a 3-D wing. For each case, a brief overview of the problem and references to previous publications are provided. The three cases are aerospace examples of the challenges and opportunities presented by optimization under uncertainty. The present paper will illustrate a variety of needs for this technology, summarize promising methods, and uncover fruitful areas for new research. C1 NASA, Langley Res Ctr, Hampton, VA 23681 USA. RP Padula, SL (reprint author), NASA, Langley Res Ctr, Mail Stop 442, Hampton, VA 23681 USA. NR 14 TC 21 Z9 21 U1 1 U2 13 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 1389-4420 J9 OPTIM ENG JI Optim. Eng. PD SEP PY 2006 VL 7 IS 3 BP 317 EP 328 DI 10.1007/s11081-006-9974-7 PG 12 WC Engineering, Multidisciplinary; Operations Research & Management Science; Mathematics, Interdisciplinary Applications SC Engineering; Operations Research & Management Science; Mathematics GA 106MF UT WOS:000242103900006 ER PT J AU Newman, N Wu, SY Liu, HX Medvedeva, J Gu, L Singh, RK Yu, ZG Krainsky, IL Krishnamurthy, S Smith, DJ Freeman, AJ van Schilfgaarde, M AF Newman, N. Wu, S. Y. Liu, H. X. Medvedeva, J. Gu, Lin Singh, R. K. Yu, Z. G. Krainsky, I. L. Krishnamurthy, S. Smith, D. J. Freeman, A. J. van Schilfgaarde, M. TI Recent progress towards the development of ferromagnetic nitride semiconductors for spintronic applications SO PHYSICA STATUS SOLIDI A-APPLICATIONS AND MATERIALS SCIENCE LA English DT Article ID MOLECULAR-BEAM EPITAXY; ROOM-TEMPERATURE; MAGNETIC SEMICONDUCTORS; SPIN POLARIZATION; THIN-FILMS; GAAS; INTERFACE; METAL; GAN; ALN AB This article describes progress towards producing prototype magnetoelectronic structures based on III-N semiconductor materials. We focus on the materials properties connected with the key physical phenomena underlying potential spintronic devices: producing, injecting, transporting, manipulating and detecting spin-polarized electron populations. Our experiments have shown that the maximum magnetic moment is realized for a composition of Ga0.97Cr0.03N and a substrate growth temperature of similar to 1050 K. Ion channeling experiments show that similar to 90% of Cr sits substitutionally on the cation site. The highest measured magnetization was 1.8 mu(B)/Cr atom (similar to 60% of the expected moment from band theory for ideal material) with the Curie temperature over similar to 900 K. This strongly suggests a link between the Cr-Ga impurity band and ferromagnetism and suggests that a double-exchange-like mechanism is responsible for the ferromagnetic ordering. The transport properties of spin-polarized charge carriers were modeled theoretically taking into account both the Elliott-Yafet and the D'yakonov-Perel' scattering mechanisms. We include the spin-orbit interaction in the unperturbed Hamiltonian and treat scattering by ionized impurities and phonons as a perturbation. Our numerical calculations predict two orders of magnitude longer electron spin relaxation times and an order of magnitude shorter hole spin relaxation times in GaN than in GaAs. First-principles electronic structure calculations predict that efficient spin injection can be achieved using a ferromagnetic GaN: Cr electrode in conjunction with an AN tunnel barrier. In this structure, the electrode is found to be half-metallic up to the interface and is thus a candidate for high-efficiency magnetoelectronic devices. (c) 2006 WILEY-VCH Verlag GmbH & Co. KGaA, Weinheim. C1 Arizona State Univ, Dept Chem & Mat Engn, Tempe, AZ 85287 USA. Northwestern Univ, Dept Phys & Astron, Evanston, IL 60208 USA. Univ Missouri, Dept Phys, Rolla, MO 65409 USA. Arizona State Univ, Ctr Solid State Sci, Tempe, AZ 85287 USA. Arizona State Univ, Dept Phys & Astron, Tempe, AZ 85287 USA. SRI Int, Menlo Pk, CA 94025 USA. NASA, Glenn Res Lab, Cleveland, OH 44135 USA. RP Newman, N (reprint author), Arizona State Univ, Dept Chem & Mat Engn, POB 876006, Tempe, AZ 85287 USA. EM nate.newman@asu.edu RI Yu, Z/B-5547-2009; Gu, Lin/F-3980-2010; Newman, Nathan/E-1466-2011; Gu, Lin/D-9631-2011; Medvedeva, Julia/F-5693-2015 OI Newman, Nathan/0000-0003-2819-9616; Gu, Lin/0000-0002-7504-031X; NR 49 TC 15 Z9 15 U1 0 U2 11 PU WILEY-V C H VERLAG GMBH PI WEINHEIM PA POSTFACH 101161, 69451 WEINHEIM, GERMANY SN 1862-6300 EI 1862-6319 J9 PHYS STATUS SOLIDI A JI Phys. Status Solidi A-Appl. Mat. PD SEP PY 2006 VL 203 IS 11 BP 2729 EP 2737 DI 10.1002/pssa.200669636 PG 9 WC Materials Science, Multidisciplinary; Physics, Applied; Physics, Condensed Matter SC Materials Science; Physics GA 088ZO UT WOS:000240849800032 ER PT J AU Lukomski, M Sutton, S Kedzierski, W Reddish, TJ Bartschat, K Bartlett, PL Bray, I Stelbovics, AT McConkey, JW AF Lukomski, M. Sutton, S. Kedzierski, W. Reddish, T. J. Bartschat, K. Bartlett, P. L. Bray, I. Stelbovics, A. T. McConkey, J. W. TI Electron-impact ionization cross sections out of the ground and 6 P-2 excited states of cesium SO PHYSICAL REVIEW A LA English DT Article ID MAGNETOOPTICAL TRAP; ATOMS; EXCITATION; THRESHOLD; RUBIDIUM; HELIUM; IONS AB An atom trapping technique for determining absolute, total ionization cross sections (TICS) out of an excited atom is presented. The unique feature of our method is in utilizing Doppler cooling of neutral atoms to determine ionization cross sections. This fluorescence-monitoring experiment, which is a variant of the "trap loss" technique, has enabled us to obtain the experimental electron impact ionization cross sections out of the Cs 6 P-2(3/2) state between 7 eV and 400 eV. CCC, RMPS, and Born theoretical results are also presented for both the ground and excited states of cesium and rubidium. In the low energy region (< 11 eV) where best agreement between these excited state measurements and theory might be expected, a discrepancy of approximately a factor of five is observed. Above this energy there are significant contributions to the TICS from both autoionization and multiple ionization. C1 Univ Windsor, Dept Phys, Windsor, ON N9B 3P4, Canada. Jagiellonian Univ, Inst Fiz, PL-30059 Krakow, Poland. Drake Univ, Dept Phys, Des Moines, IA 50311 USA. Murdoch Univ, ARC Ctr Antimatter Matter Studies, Perth, WA, Australia. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Reddish, TJ (reprint author), Univ Windsor, Dept Phys, Windsor, ON N9B 3P4, Canada. EM reddish@uwindsor.ca; mcconk@uwindsor.ca RI Bray, Igor/B-8586-2009; Bartschat, Klaus/I-2527-2012; OI Bray, Igor/0000-0001-7554-8044; Lukomski, Michal/0000-0001-7942-9026 NR 28 TC 20 Z9 20 U1 4 U2 12 PU AMERICAN 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 SEP PY 2006 VL 74 IS 3 AR 032708 DI 10.1103/PhysRevA.74.032708 PG 6 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA 091ZP UT WOS:000241067100079 ER PT J AU Choi, DS Kopczyk, M Kayani, A Smith, RJ Bozzolo, G AF Choi, D. S. Kopczyk, M. Kayani, A. Smith, R. J. Bozzolo, Guillermo TI Structure of ultrathin Ag films on the Al(100) surface SO PHYSICAL REVIEW B LA English DT Article ID ENERGY ION-SCATTERING; SINGLE-CRYSTAL SURFACES; ELECTRONIC-STRUCTURE; GROWTH; SPECTROSCOPY; AL(111); STATES; FACES; PHASE; AU AB The structure for submonolayer amounts of Ag deposited on the Al(100) surface at room temperature has been studied using low-energy electron diffraction (LEED) and low-energy ion-scattering spectroscopy (LEIS/ISS). The Ag coverage was determined using Rutherford backscattering spectroscopy. We conclude that the Ag atoms form two domains of a buckled, quasihexagonal coincident lattice structure on the Al(100) surface, having a repeat distance of 5 Al interatomic spacings in the [110] direction. The LEED pattern shows a double-domain (5x1) structure with additional intensity in those spots corresponding to a (111) close-packed hexagonal layer. The analysis of the ISS results suggests that the heights of the adsorbed Ag atoms above the Al surface are not all the same, leading to the proposed buckling model that is in agreement with recent scanning tunneling microscopy measurements. In addition, some Al atoms move from the substrate up into the Ag adlayer to form a surface alloy. Model calculations using the quantum approximate Bozzolo-Ferrante-Smith (BFS) method indicate that the hexagonal layer is energetically preferred as a result of increased nearest-neighbor coordination within the Ag layer. C1 Kangweon Natl Univ, Dept Phys, Chunchon 200701, South Korea. Montana State Univ, Dept Phys, Bozeman, MT 59717 USA. Ohio Aerosp Inst, Cleveland, OH 44142 USA. NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. RP Choi, DS (reprint author), Kangweon Natl Univ, Dept Phys, Chunchon 200701, South Korea. NR 31 TC 6 Z9 6 U1 2 U2 7 PU AMERICAN 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 SEP PY 2006 VL 74 IS 11 AR 115407 DI 10.1103/PhysRevB.74.115407 PG 8 WC Physics, Condensed Matter SC Physics GA 089HV UT WOS:000240872300105 ER PT J AU Lawson, JW Bauschlicher, CW AF Lawson, John W. Bauschlicher, Charles W., Jr. TI Transport in molecular junctions with different metallic contacts SO PHYSICAL REVIEW B LA English DT Article ID CURRENT-VOLTAGE CURVES; LOCALIZED SCATTERERS; ELECTRONIC DEVICES; SPATIAL VARIATION; SINGLE MOLECULES; CONDUCTANCE; WIRES; FORMALISM; SURFACES; CURRENTS AB Ab initio calculations of phenyl dithiol connected to Au, Ag, Pd, and Pt electrodes are performed using nonequilibrium Green's functions and density functional theory. For each metal, the properties of the molecular junction are considered both in equilibrium and under bias. In particular, we consider in detail charge transfer, changes in the electrostatic potential, and their subsequent effects on the I-V curves through the junctions. Gold is typically used in molecular junctions because it forms strong chemical bonds with sulfur. We find, however, that Pt and Pd make better electrical contacts than Au. The zero-bias conductance is found to be greatest for Pt, followed by Pd, Au, and then Ag. C1 NASA, Ames Res Ctr, Ctr Nanotechnol, Moffett Field, CA 94035 USA. RP Lawson, JW (reprint author), NASA, Ames Res Ctr, Ctr Nanotechnol, Mail Stop 269-2, Moffett Field, CA 94035 USA. EM john.w.lawson@nasa.gov; Charles.W.Bauschlicher@nasa.gov NR 41 TC 28 Z9 28 U1 1 U2 7 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 SEP PY 2006 VL 74 IS 12 AR 125401 DI 10.1103/PhysRevB.74.125401 PG 8 WC Physics, Condensed Matter SC Physics GA 089HX UT WOS:000240872500072 ER PT J AU Mingo, N AF Mingo, N. TI Anharmonic phonon flow through molecular-sized junctions SO PHYSICAL REVIEW B LA English DT Article ID THERMAL-CONDUCTIVITY; MESOSCOPIC SYSTEMS; HEAT-FLOW; LATTICE; QUANTUM; CONDUCTANCE; SIMULATION; RESISTANCE; TRANSPORT; DYNAMICS AB A general many-body nonequilibrium Green's function approach for interacting phonons is developed, and applied to study the thermal conductance of an anharmonic molecular junction between two solid surfaces. We investigate the dependence of the nanojunction's thermal conductance on temperature, force constants, and bond anharmonicity, and identify different parameter regimes. The calculation results display quantum mechanical effects that differ significantly from classical predictions. The anharmonic technique presented extends the scope of fully quantum mechanical Green's function calculations of phonon transport, which until now had been largely restricted to harmonic (or noninteracting phonon) systems. Thus it may provide a powerful tool for the study of lattice thermal conduction in nanoscale systems, such as point contacts, molecular contacts, and interfaces. C1 NASA, Ames Ctr Nanotechnol, Moffett Field, CA 94035 USA. RP Mingo, N (reprint author), NASA, Ames Ctr Nanotechnol, N229-1, Moffett Field, CA 94035 USA. NR 54 TC 131 Z9 131 U1 1 U2 25 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 2469-9950 EI 2469-9969 J9 PHYS REV B JI Phys. Rev. B PD SEP PY 2006 VL 74 IS 12 AR 125402 DI 10.1103/PhysRevB.74.125402 PG 13 WC Physics, Condensed Matter SC Physics GA 089HX UT WOS:000240872500073 ER PT J AU Misner, CW van Meter, JR Fiske, DR AF Misner, Charles W. van Meter, James R. Fiske, David R. TI Excising das all: Evolving maxwell waves beyond scri SO PHYSICAL REVIEW D LA English DT Article ID MESH REFINEMENT; BLACK-HOLES; RELATIVITY AB We study the numerical propagation of waves through future null infinity in a conformally compactified spacetime. We introduce an artificial cosmological constant, which allows us some control over the causal structure near null infinity. We exploit this freedom to ensure that all light cones are tilted outward in a region near null infinity, which allows us to impose excision-style boundary conditions in our finite-difference code. In this preliminary study we consider electromagnetic waves propagating in a static, conformally compactified spacetime. C1 Univ Maryland, Dept Phys, College Pk, MD 20742 USA. Max Planck Inst Gravitationsphys, Albert Einstein Inst, D-14476 Potsdam, Germany. Decis Analyt Cor, Intelligent Syst Div, Arlington, VA 22202 USA. NASA, Goddard Space Flight Ctr, Lab Gravitat Astrophys, Greenbelt, MD 20771 USA. RP Misner, CW (reprint author), Univ Maryland, Dept Phys, College Pk, MD 20742 USA. RI van meter, james/E-7893-2011 NR 31 TC 0 Z9 0 U1 0 U2 0 PU AMERICAN 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 SEP PY 2006 VL 74 IS 6 AR 064003 DI 10.1103/PhysRevD.74.064003 PG 10 WC Astronomy & Astrophysics; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA 089IR UT WOS:000240874500044 ER PT J AU Obreschkow, D Kobel, P Dorsaz, N de Bosset, A Nicollier, C Farhat, M AF Obreschkow, D. Kobel, P. Dorsaz, N. de Bosset, A. Nicollier, C. Farhat, M. TI Cavitation bubble dynamics inside liquid drops in microgravity SO PHYSICAL REVIEW LETTERS LA English DT Article ID FREE-SURFACE; RIGID BOUNDARY; COLLAPSE AB We studied spark-generated cavitation bubbles inside water drops produced in microgravity. High-speed visualizations disclosed unique effects of the spherical and nearly isolated liquid volume. In particular, (1) toroidally collapsing bubbles generate two liquid jets escaping from the drop, and the "splash jet" discloses a remarkable broadening. (2) Shock waves induce a strong form of secondary cavitation due to the particular shock wave confinement. This feature offers a novel way to estimate integral shock wave energies in isolated volumes. (3) Bubble lifetimes in drops are shorter than in extended volumes in remarkable agreement with herein derived corrective terms for the Rayleigh-Plesset equation. C1 Ecole Polytech Fed Lausanne, Lab Machines Hydraul, CH-1007 Lausanne, Switzerland. Univ Oxford, Dept Phys, Oxford OX1 3PU, England. Max Planck Inst Solar Syst Res, D-37191 Katlenburg Lindau, Germany. Ecole Polytech Fed Lausanne, Inst Romand Rech Numer Phys Mat, CH-1015 Lausanne, Switzerland. NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. ESA, European Astronaut Ctr, Cologne, Germany. RP Obreschkow, D (reprint author), Ecole Polytech Fed Lausanne, Lab Machines Hydraul, CH-1007 Lausanne, Switzerland. RI Farhat, Mohamed/H-9463-2012 OI Farhat, Mohamed/0000-0002-4782-2170 NR 18 TC 42 Z9 46 U1 2 U2 28 PU AMERICAN 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 SEP 1 PY 2006 VL 97 IS 9 AR 094502 DI 10.1103/PhysRevLett.97.094502 PG 4 WC Physics, Multidisciplinary SC Physics GA 080HR UT WOS:000240239000026 PM 17026369 ER PT J AU Birn, J Hesse, M Schindler, K AF Birn, J. Hesse, M. Schindler, K. TI Entropy conservation in simulations of magnetic reconnection SO PHYSICS OF PLASMAS LA English DT Article ID ELECTRON DISSIPATION; FIELD; DYNAMICS; PLASMA; LINE AB Entropy and mass conservation are investigated for the dynamic field evolution associated with fast magnetic reconnection, based on the "Newton Challenge" problem [Birn , Geophys. Res. Lett. 32, L06105 (2005)]. In this problem, the formation of a thin current sheet and magnetic reconnection are initiated in a plane Harris-type current sheet by temporally limited, spatially varying, inflow of magnetic flux. Using resistive magnetohydrodynamic (MHD) and particle-in-cell (PIC) simulations, specifically the entropy and mass integrated along the magnetic flux tubes are compared between the simulations. In the MHD simulation these should be exactly conserved quantities, when slippage and Ohmic dissipation are negligible. It is shown that there is very good agreement between the conservation of these quantities in the two simulation approaches, despite the effects of dissipation, provided that the resistivity in the MHD simulation is strongly localized. This demonstrates that dissipation is highly localized in the PIC simulation also, and that heat flux across magnetic flux tubes has negligible effect as well, so that the entropy increase on a full flux tube remains small even during reconnection. The mass conservation also implies that the frozen-in flux condition of ideal MHD is a good integral approximation outside the reconnection site. This result lends support for using the entropy-conserving MHD approach not only before and after reconnection but even as a constraint connecting the two phases. (c) 2006 American Institute of Physics. C1 Los Alamos Natl Lab, Los Alamos, NM 87545 USA. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Ruhr Univ Bochum, Inst Theoret Phys, D-44780 Bochum, Germany. RP Birn, J (reprint author), Los Alamos Natl Lab, POB 1663, Los Alamos, NM 87545 USA. EM jbirn@lanl.gov RI Hesse, Michael/D-2031-2012; NASA MMS, Science Team/J-5393-2013 OI NASA MMS, Science Team/0000-0002-9504-5214 NR 18 TC 23 Z9 23 U1 0 U2 2 PU AMER INST PHYSICS PI MELVILLE PA CIRCULATION & FULFILLMENT DIV, 2 HUNTINGTON QUADRANGLE, STE 1 N O 1, MELVILLE, NY 11747-4501 USA SN 1070-664X J9 PHYS PLASMAS JI Phys. Plasmas PD SEP PY 2006 VL 13 IS 9 AR 092117 DI 10.1063/1.2349440 PG 6 WC Physics, Fluids & Plasmas SC Physics GA 089JX UT WOS:000240877800018 ER PT J AU Smith, TM Nelson, GL AF Smith, Trent M. Nelson, Gordon L. TI Ferrocene containing copolymers with improved electrostatic dissipation properties for advanced applications SO POLYMERS FOR ADVANCED TECHNOLOGIES LA English DT Article; Proceedings Paper CT 8th International Symposium on Polymers for Advanced Technologies CY SEP 13-16, 2005 CL Budapest, HUNGARY SP IUPAC, European Polymer Federat, Soc Polymer Sci Japan, Chem Soc Japan, Amer Chem Soc, Polymer & PMSE Div, Hungarian Acad Sci, Budapest Univ Technol & Econ DE electrostatic charge dissipation; ferrocene polymers; block copolymers; polyurethanes; oligomers AB Polyurethane (PU) and polyimide (PI) copolymers containing a ferrocene oligomer (FcOlig) in the backbone were synthesized and characterized. PU materials with the FcOlig in the chain (PU-FcOlig) demonstrated improved electrostatic dissipation properties and decreased electrical resistance in comparison to the unmodified PU parent material. The surface resistance decreased nearly 30 times and the volume resistance decreased nearly 12 times with a 3.5% FcOlig reacted in with Rubinate (R) 9272. The same 3.5% PU-FcOlig material exhibited an average surface potential resulting from charge deposited of 130 +/- 4 V down from 1600 +/- 65 V for the unmodified PU. The charge dissipation time to 1/e (initial voltage divided by e) was also decreased to 81 +/- 7 msec for 1.5% PU-FcOlig materials from an average of 934 +/- 62 msec for the parent PU. Incorporating the FcOlig into the backbone of a PI (BPDA-ODA PI FcOlig) had no significant effects on the electrical properties in comparison to the unmodified parent PI (BPDA, 3,3 ', 4,4 '-biphenyltetracarboxylic dianhydride; ODA, 3,3 '-oxydianiline). The difference in electrical properties between the ferrocene containing PUs and PIs is the lack of FcOlig blocks on or near the surface of the PI. X-ray photoelectron spectroscopy (XPS) confirms that on the surface of the ferrocene containing PUs iron in the form of ferrocene is detected, but even after etching the PIs to a depth of 50, 100, 50 angstrom, and finally scraping the surface with a scalpel no iron was observed. Published in 2006 by John Wiley & Sons, Ltd. C1 Florida Inst Technol, Melbourne, FL 32901 USA. NASA, Spaceport Technol Div, Kennedy Space Ctr, FL 32899 USA. RP Nelson, GL (reprint author), Florida Inst Technol, 150 W Univ Blvd, Melbourne, FL 32901 USA. EM nelson@fit.edu NR 17 TC 8 Z9 8 U1 1 U2 8 PU JOHN WILEY & SONS LTD PI CHICHESTER PA THE ATRIUM, SOUTHERN GATE, CHICHESTER PO19 8SQ, W SUSSEX, ENGLAND SN 1042-7147 J9 POLYM ADVAN TECHNOL JI Polym. Adv. Technol. PD SEP-OCT PY 2006 VL 17 IS 9-10 BP 746 EP 753 DI 10.1002/pat.780 PG 8 WC Polymer Science SC Polymer Science GA 117PG UT WOS:000242884700022 ER PT J AU Lien, MC Allen, PA Ruthruff, E Grabbe, J McCann, RS Remington, RW AF Lien, Mei-Ching Allen, Philip A. Ruthruff, Eric Grabbe, Jeremy McCann, Robert S. Remington, Roger W. TI Visual word recognition without central attention: Evidence for greater automaticity with advancing age SO PSYCHOLOGY AND AGING LA English DT Article DE aging; dual-task interference; visual word recognition; divided attention ID PSYCHOLOGICAL REFRACTORY-PERIOD; DUAL-TASK INTERFERENCE; CHRONOMETRIC EVIDENCE; RESPONSE SELECTION; OVERLAPPING TASKS; OLDER ADULTS; PERFORMANCE; BOTTLENECK; STROOP; LOCUS AB The present experiments examined the automaticity of word recognition. The authors examined whether people can recognize words while central attention is devoted to another task and how this ability changes across the life span. In Experiment 1, a lexical decision Task 2 was combined with either an auditory or a visual Task 1. Regardless of the Task 1 modality, Task 2 word recognition proceeded in parallel with Task 1 central operations for older adults but not for younger adults. This is a rare example of improved cognitive processing with advancing age. When Task 2 was nonlexical (Experiment 2), however, there was no evidence for greater parallel processing for older adults. Thus, the processing advantage appears to be restricted to lexical processes. The authors conclude that greater cumulative experience with lexical processing leads to greater automaticity, allowing older adults to more efficiently perform this stage in parallel with another task. C1 Oregon State Univ, Dept Psychol, Corvallis, OR 97331 USA. Univ Akron, Dept Psychol, Akron, OH 44325 USA. Univ New Mexico, Dept Psychol, Albuquerque, NM 87131 USA. Natl Aeronaut & Space Adm, Ames Res Ctr, Moffett Field, CA USA. Johns Hopkins Univ, Appl Phys Lab, Baltimore, MD 21287 USA. RP Lien, MC (reprint author), Oregon State Univ, Dept Psychol, Corvallis, OR 97331 USA. EM mei.lien@oregonstate.edu OI Allen, Philip/0000-0001-8567-2217 NR 46 TC 39 Z9 39 U1 5 U2 14 PU AMER PSYCHOLOGICAL ASSOC/EDUCATIONAL PUBLISHING FOUNDATION PI WASHINGTON PA 750 FIRST ST NE, WASHINGTON, DC 20002-4242 USA SN 0882-7974 J9 PSYCHOL AGING JI Psychol. Aging PD SEP PY 2006 VL 21 IS 3 BP 431 EP 447 DI 10.1037/0882-7974.21.3.431 PG 17 WC Gerontology; Psychology, Developmental SC Geriatrics & Gerontology; Psychology GA 083LE UT WOS:000240456600001 PM 16953708 ER PT J AU Bozorgnia, N Fortney, JJ McCarthy, C Fischer, DA Marcy, GW AF Bozorgnia, Nassim Fortney, Jonathan J. McCarthy, Chris Fischer, Debra A. Marcy, Geoffrey W. TI The search for an atmospheric signature of the transiting exoplanet HD 149026b SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF THE PACIFIC LA English DT Article ID GIANT PLANET ATMOSPHERES; TRANSMISSION SPECTRA; EXTRASOLAR; SODIUM; DWARF; CORE AB HD 149026b is a short-period, Saturn-mass planet that transits a metal-rich star. The planet's radius, determined by photometry, is remarkably small compared to other known transiting planets, with a heavy-element core that apparently comprises similar to 70% of the total planet mass. Time-series spectra were obtained at Keck before and during transit in order to model the Rossiter-McLaughlin effect. Here we make use of these observations to carry out a differential comparison of spectra obtained in and out of transit to search for signatures of neutral atomic lithium and potassium from the planet atmosphere. No signal was detected at the 2% level; we therefore place upper limits on the column density of these atoms. C1 San Francisco State Univ, Dept Phys & Astron, San Francisco, CA 94132 USA. NASA, Ames Res Ctr, Space Sci & Astrobiol Div, Moffett Field, CA 94035 USA. SETI Inst, Mountain View, CA 94043 USA. Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. RP Bozorgnia, N (reprint author), San Francisco State Univ, Dept Phys & Astron, 1600 Holloway Ave, San Francisco, CA 94132 USA. EM jfortney@arc.nasa.gov; fischer@stars.sfsu.edu NR 25 TC 3 Z9 3 U1 2 U2 2 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-6280 EI 1538-3873 J9 PUBL ASTRON SOC PAC JI Publ. Astron. Soc. Pac. PD SEP PY 2006 VL 118 IS 847 BP 1252 EP 1259 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 091GT UT WOS:000241015800005 ER PT J AU Catanzarite, J Shao, M Tanner, A Unwin, S Yu, J AF Catanzarite, Joseph Shao, Michael Tanner, Angelle Unwin, Stephen Yu, Jeffrey TI Astrometric detection of terrestrial planets in the habitable zones of nearby stars with SIM PlanetQuest SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF THE PACIFIC LA English DT Article ID SPACE-INTERFEROMETRY-MISSION; NARROW-ANGLE ASTROMETRY; NEPTUNE-MASS PLANET; EXTRASOLAR PLANETS; TIME-SERIES; SEARCH; DETECTABILITY; COMPANIONS; EXOPLANETS; SYSTEMS AB SIM PlanetQuest (formerly the Space Interferometry Mission) is a space-borne Michelson interferometer for precision stellar astrometry, with a 9 m baseline, currently slated for launch in 2016. One of the principal science goals is the astrometric detection and orbital characterization of terrestrial planets in the habitable zones of nearby stars. Differential astrometry of the target star against a set of reference stars lying within 1 degrees will allow measurement of the target star's reflex motion with astrometric accuracy of 1 mu as in a single measurement. The purpose of the present paper is to quantitatively assess SIM's capability for detection (as opposed to characterization by orbital determination) of terrestrial planets in the habitable zones of nearby stars. Note that the orbital periods of these planets are generally shorter than the 5 year SIM mission. We formulate a "joint periodogram" as a tool for planet detection from astrometric data. For adequately sampled orbits (i.e., five or more observations per period over a sampling time span longer than the orbital period), we find that the joint periodogram is more sensitive than the chi(2) test for the null hypothesis. In our analysis 2 of the problem, we use Monte Carlo simulations of orbit detection, together with realistic observing scenarios, actual target and reference star lists, realistic estimates of SIM instrument performance, and plausible distributions of planetary system parameters. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Catanzarite, J (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM jcat@s383.jpl.nasa.gov NR 32 TC 2 Z9 3 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 SEP PY 2006 VL 118 IS 847 BP 1322 EP 1342 PG 21 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 091GT UT WOS:000241015800008 ER PT J AU Yin, XC Mora, P Donnellan, A Matsuura, M AF Yin, Xiang-Chu Mora, Peter Donnellan, Andrea Matsuura, Mitsuhiro TI Computational earthquake physics - PART I: Introduction SO PURE AND APPLIED GEOPHYSICS LA English DT Editorial Material ID SCIENCE C1 Chinese Earthquake Adm, Inst Earthquake Sci, Beijing 100036, Peoples R China. Chinese Acad Sci, Inst Mech, State Key Lab Nonlinear Mech, Beijing 100080, Peoples R China. Univ Queensland, Earth Syst Sci Computat Ctr, Brisbane, Qld 4072, Australia. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. Univ Tokyo, Dept Earth & Planetary Sci, Bunkyo Ku, Tokyo 1130033, Japan. RP Yin, XC (reprint author), Chinese Earthquake Adm, Inst Earthquake Sci, Beijing 100036, Peoples R China. EM xcyin@public.bta.net.cn; director@esscc.uq.edu.au; andrea.donnellan@jpl.nasa.gov; matsuura@eps.s.u-tokyo.ac.jp NR 6 TC 2 Z9 2 U1 0 U2 0 PU BIRKHAUSER VERLAG AG PI BASEL PA VIADUKSTRASSE 40-44, PO BOX 133, CH-4010 BASEL, SWITZERLAND SN 0033-4553 J9 PURE APPL GEOPHYS JI Pure Appl. Geophys. PD SEP PY 2006 VL 163 IS 9 BP 1737 EP 1740 DI 10.1007/s00024-006-0112-4 PG 4 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 097NU UT WOS:000241455500001 ER PT J AU Rundle, PB Rundle, JB Tiampo, KF Donnellan, A Turcotte, DL AF Rundle, P. B. Rundle, J. B. Tiampo, K. F. Donnellan, A. Turcotte, D. L. TI Virtual California: Fault model, frictional parameters, applications SO PURE AND APPLIED GEOPHYSICS LA English DT Article; Proceedings Paper CT 4th ACES Workshop 2004 CY JUL 09-14, 2004 CL Beijing, PEOPLES R CHINA DE earthquakes; simulations; fault Systems; forecasting; statistics ID SYNTHETIC SEISMICITY MODEL; SAN-ANDREAS FAULT; SOUTHERN-CALIFORNIA; ROCK FRICTION; EARTHQUAKES; SIMULATIONS; EVOLUTION; AREA AB Virtual California is a topologically realistic simulation of the interacting earthquake faults in California. Inputs to the model arise from field data, and typically include realistic fault system topologies, realistic long-term slip rates, and realistic frictional parameters. Outputs from the simulations include synthetic earthquake sequences and space-time patterns together with associated surface deformation and strain patterns that are similar to those seen in nature. Here we describe details of the data assimilation procedure we use to construct the fault model and to assign frictional properties. In addition, by analyzing the statistical physics of the simulations, we can show that that the frictional failure physics, which includes a simple representation of a dynamic stress intensity factor, leads to self-organization of the statistical dynamics, and produces empirical statistical distributions (probability density functions: PDFs) that characterize the activity. One type of distribution that can be constructed from empirical measurements of simulation data are PDFs for recurrence intervals on selected faults. Inputs to simulation dynamics are based on the use of time-averaged event-frequency data, and outputs include PDFs representing measurements of dynamical variability arising from fault interactions and space-time correlations. As a first step for productively using model-based methods for earthquake forecasting, we propose that simulations be used to generate the PDFs for recurrence intervals instead of the usual practice of basing the PDFs on standard forms (Gaussian, Log-Normal, Pareto, Brownian Passage Time, and so forth). Subsequent development of simulation-based methods should include model enhancement, data assimilation and data mining methods, and analysis techniques based on statistical physics. C1 Univ Calif Davis, Ctr Computat Sci & Engn, Davis, CA 95616 USA. Univ Calif Davis, Dept Phys, Davis, CA 95616 USA. Univ Calif Davis, Dept Engn, Davis, CA 95616 USA. Univ Western Ontario, Dept Earth Sci, London, ON, Canada. Jet Propuls Lab, Div Earth & Space Sci, Pasadena, CA USA. Univ Calif Davis, Dept Geol, Davis, CA 95616 USA. RP Rundle, PB (reprint author), Univ Calif Davis, Ctr Computat Sci & Engn, Davis, CA 95616 USA. EM prundle@cse.ucdavis.edu; jbrundle@ucdavis.edu; ktiampo@uwo.ca; andrea.donnellan@jpl.nasa.gov; turcotte@geology.ucdavis.edu RI Tiampo, Kristy/I-1355-2015 OI Tiampo, Kristy/0000-0002-5500-7600 NR 29 TC 36 Z9 37 U1 0 U2 3 PU BIRKHAUSER VERLAG AG PI BASEL PA VIADUKSTRASSE 40-44, PO BOX 133, CH-4010 BASEL, SWITZERLAND SN 0033-4553 J9 PURE APPL GEOPHYS JI Pure Appl. Geophys. PD SEP PY 2006 VL 163 IS 9 BP 1819 EP 1846 DI 10.1007/s00024-006-0099-x PG 28 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 097NU UT WOS:000241455500007 ER PT J AU Gaza, R Yukihara, EG McKeever, SWS AF Gaza, R. Yukihara, E. G. McKeever, S. W. S. TI The use of optically stimulated luminescence from AL(2)O(3): C in the dosimetry of high-energy heavy charged particle fields SO RADIATION PROTECTION DOSIMETRY LA English DT Article ID AL2O3-C AB This paper presents two different approaches of quantifying the optically stimulated luminescence (OSL) response of Al2O3:C to high-energy heavy charged particles (HCPs). The OSL efficiency of Al2O3:C exposed to different HCPs is defined as the sensitivity of the material to HCPs normalised by the sensitivity to gamma. In this paper, we investigate the possibility of introducing a 'mean efficiency' eta(mean), which when used in conjunction with the total gamma dose D-gamma measured for a mixed radiation exposure allows for the determination of the absorbed dose without the need to determine the individual contributions of different types of radiation to the OSL signal. We tested the hypothesis that information regarding the 'mean efficiency' eta(mean) is contained in the shape of the OSL decay curve, using several approaches in the analysis of the OSL data. This analysis was applied to various mixed field irradiations performed at the HIMAC facility, Chiba, Japan. The results of this analysis are discussed. C1 Oklahoma State Univ, Dept Phys, Stillwater, OK 74078 USA. RP Gaza, R (reprint author), NASA, Lyndon B Johnson Space Ctr, Space Radiat Anal Grp, 2101 NASA Pkwy, Houston, TX 77058 USA. EM ramona.gaza-1@nasa.gov RI Yukihara, Eduardo/F-1345-2014 OI Yukihara, Eduardo/0000-0002-4615-6698 NR 8 TC 5 Z9 5 U1 1 U2 4 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0144-8420 J9 RADIAT PROT DOSIM JI Radiat. Prot. Dosim. PD SEP PY 2006 VL 120 IS 1-4 BP 354 EP 357 DI 10.1093/rpd/nci574 PG 4 WC Environmental Sciences; Public, Environmental & Occupational Health; Nuclear Science & Technology; Radiology, Nuclear Medicine & Medical Imaging SC Environmental Sciences & Ecology; Public, Environmental & Occupational Health; Nuclear Science & Technology; Radiology, Nuclear Medicine & Medical Imaging GA 086RZ UT WOS:000240692000073 PM 16644985 ER PT J AU Pisacane, VL Ziegler, JF Nelson, ME Caylor, M Flake, D Heyen, L Youngborg, E Rosenfeld, AB Cucinotta, F Zaider, M Dicello, JF AF Pisacane, V. L. Ziegler, J. F. Nelson, M. E. Caylor, M. Flake, D. Heyen, L. Youngborg, E. Rosenfeld, A. B. Cucinotta, F. Zaider, M. Dicello, J. F. TI MIDN: A spacecraft microdosimeter mission SO RADIATION PROTECTION DOSIMETRY LA English DT Article AB MIDN (MIcroDosimetry iNstrument) is a payload on the MidSTAR-I spacecraft (Midshipman Space Technology Applications Research) under development at the United States Naval Academy. MIDN is a solid-state system being designed and constructed to measure microdosimetric spectra to determine radiation quality factors for space environments. Radiation is a critical threat to the health of astronauts and to the success of missions in low-Earth orbit and space exploration. The system will consist of three separate sensors, one external to the spacecraft, one internal and one embedded in polyethylene. Design goals are mass < 3 kg and power < 2 W. The MidSTAR-I mission in 2006 will provide an opportunity to evaluate a preliminary version of this system. Its low power and mass makes it useful for the International Space Station and manned and unmanned interplanetary missions as a real-time system to assess and alert astronauts to enhanced radiation environments. C1 Johns Hopkins Univ, Sch Med, Baltimore, MD 21231 USA. USN Acad, Annapolis, MD 21402 USA. Univ Wollongong, Wollongong, NSW 2522, Australia. NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. Mem Sloan Kettering Canc Ctr, New York, NY 10021 USA. RP Dicello, JF (reprint author), Johns Hopkins Univ, Sch Med, Baltimore, MD 21231 USA. EM ltheyen@yahoo.com; anatoly@uow.edu.au; diceljo@jhmi.edu RI Rosenfeld, Anatoly/D-1989-2014; OI Zaider, Marco/0000-0002-5113-7862 NR 12 TC 2 Z9 2 U1 0 U2 3 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0144-8420 J9 RADIAT PROT DOSIM JI Radiat. Prot. Dosim. PD SEP PY 2006 VL 120 IS 1-4 BP 421 EP 426 DI 10.1093/rpd/nci601 PG 6 WC Environmental Sciences; Public, Environmental & Occupational Health; Nuclear Science & Technology; Radiology, Nuclear Medicine & Medical Imaging SC Environmental Sciences & Ecology; Public, Environmental & Occupational Health; Nuclear Science & Technology; Radiology, Nuclear Medicine & Medical Imaging GA 086RZ UT WOS:000240692000087 PM 16785245 ER PT J AU Gaza, R Yukihara, EG McKeever, SWS Avila, O Buenfil, AE Gamboa-deBuen, I Rodriguez-Villafuerte, M Ruiz-Trejo, C Brandan, ME AF Gaza, Ramona Yukihara, Eduardo G. McKeever, Stephen W. S. Avila, Olga Buenfil, Ana-Elena Gamboa-deBuen, Isabel Rodriguez-Villafuerte, Mercedes Ruiz-Trejo, Cesar Brandan, Maria-Ester TI Ionisation density dependence of the optically stimulated luminescence dose-response of Al2O3 : C to low-energy charged particles SO RADIATION PROTECTION DOSIMETRY LA English DT Article; Proceedings Paper CT 14th International Conference on Solid State Dosimetry CY JUN 27-JUL 02, 2004 CL New Haven, CT SP Yale Univ Sch Med, Int Org Solid State Dosimetry, Oxford Univ Press, Landauer Inc, Canberra Ind, Global Dosimetry Solut Inc ID THERMO-LUMINESCENCE; THERMOLUMINESCENCE; IRRADIATION; DOSIMETRY; IONS AB The optically stimulated luminescence (OSL) response of Al2O3:C to high doses of gamma or beta irradiation can be used to predict the response of this material to charged particles as a function of particle fluence, particle energy and/or linear energy transfer (LET). In particular, it is predicted that track interaction effects at high particle fluences should result in linear-sublinear growth of the OSL signal. Similar considerations also predict a dependence of the fluence at which sublinearity starts upon the energy of the particles. In this work the OSL response of Al2O3:C to low-energy charged particles was investigated using protons (1, 2 and 4 MeV), carbon ions (13 MeV) and oxygen ions (10 MeV). The sublinear growth predicted above was qualitatively confirmed, but the energy dependence prediction was not. Furthermore, the efficiency of OSL production in the material after charged particle irradiation, compared to that obtained for gamma irradiation, is determined from the dose-response curves by fitting to a simple saturating exponential function. The efficiency values so obtained using this method are compared with those obtained from a conventional single-point measurement in the linear portion of the curve and found to be in good agreement. In general, the efficiency decreases as the LET of the particle increases. The present data are compared with published data obtained using high-energy charged particles and the results show that the efficiency is not a unique function of LET. C1 Oklahoma State Univ, Dept Phys, Stillwater, OK 74078 USA. Inst Nacl Invest Nucl, Mexico City 11801, DF, Mexico. Univ Nacl Autonoma Mexico, Inst Fis, Mexico City 01000, DF, Mexico. Univ Nacl Autonoma Mexico, Inst Ciencias Nucl, Mexico City 04510, DF, Mexico. RP Gaza, R (reprint author), NASA, Lyndon B Johnson Space Ctr, Space Radiat Anal Grp, 2101 NASA Pkwy, Houston, TX 77058 USA. EM ramona.gaza-1@nasa.gov RI Brandan, Maria-Ester/K-9014-2012; Yukihara, Eduardo/F-1345-2014 OI Brandan, Maria-Ester/0000-0002-1165-3440; Yukihara, Eduardo/0000-0002-4615-6698 NR 8 TC 5 Z9 5 U1 2 U2 6 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0144-8420 J9 RADIAT PROT DOSIM JI Radiat. Prot. Dosim. PD SEP PY 2006 VL 119 IS 1-4 BP 375 EP 379 DI 10.1093/rpd/nci545 PG 5 WC Environmental Sciences; Public, Environmental & Occupational Health; Nuclear Science & Technology; Radiology, Nuclear Medicine & Medical Imaging SC Environmental Sciences & Ecology; Public, Environmental & Occupational Health; Nuclear Science & Technology; Radiology, Nuclear Medicine & Medical Imaging GA 086RQ UT WOS:000240691100080 PM 16644998 ER PT J AU Harding, AK Lai, D AF Harding, Alice K. Lai, Dong TI Physics of strongly magnetized neutron stars SO REPORTS ON PROGRESS IN PHYSICS LA English DT Review ID X-RAY PULSAR; EQUATION-OF-STATE; SOFT GAMMA-REPEATERS; DENSITY-FUNCTIONAL CALCULATIONS; LOW-LUMINOSITY ACCRETION; CYCLOTRON RESONANT SCATTERING; PHASE-RESOLVED SPECTROSCOPY; RAPIDLY SPINNING PULSARS; BROAD ABSORPTION FEATURE; CRUSTAL PLATE-TECTONICS AB There has recently been growing evidence for the existence of neutron stars possessing magnetic fields with strengths that exceed the quantum critical field strength of 4.4 x 10(13) G, at which the cyclotron energy equals the electron rest mass. Such evidence has been provided by new discoveries of radio pulsars having very high spin-down rates and by observations of bursting gamma-ray sources termed magnetars. This paper will discuss the exotic physics of this high-field regime, where a new array of processes becomes possible and even dominant and where familiar processes acquire unusual properties. We review the physical processes that are important in neutron star interiors and magnetospheres, including the behaviour of free particles, atoms, molecules, plasma and condensed matter in strong magnetic fields, photon propagation in magnetized plasmas, free-particle radiative processes, the physics of neutron star interiors and field evolution and decay mechanisms. Application of such processes in astrophysical source models, including rotation-powered pulsars, soft gamma- ray repeaters, anomalous x-ray pulsars and accreting x-ray pulsars will also be discussed. Throughout this review, we will highlight the observational signatures of high magnetic field processes, as well as the theoretical issues that remain to be understood. C1 NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Cornell Univ, Ctr Radiophys & Space Res, Dept Astron, Ithaca, NY 14853 USA. RP Harding, AK (reprint author), NASA, Goddard Space Flight Ctr, Code 663, Greenbelt, MD 20771 USA. EM Alice.K.Harding@nasa.gov; dong@astro.cornell.edu RI Harding, Alice/D-3160-2012 NR 428 TC 368 Z9 371 U1 0 U2 17 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 SEP PY 2006 VL 69 IS 9 BP 2631 EP 2708 DI 10.1088/0034-4885/69/9/R03 PG 78 WC Physics, Multidisciplinary SC Physics GA 077EW UT WOS:000240011700003 ER PT J AU Kharuk, VI Ranson, KJ Im, ST Naurzbaev, MM AF Kharuk, V. I. Ranson, K. J. Im, S. T. Naurzbaev, M. M. TI Forest-tundra larch forests and climatic trends SO RUSSIAN JOURNAL OF ECOLOGY LA English DT Article DE larch forests; climatic trends; radial tree increment; remote sensing ID GROWTH; ALASKA AB Climate-related changes that occurred in the Ary-Mas larch forests (the world's northernmost forest range) in the last three decades of the 20th century have been analyzed. An analysis of remote-sensing images made by Landsat satellites in 1973 and 2000 has provided evidence for an increase in the closeness of larch forest canopy (by 65%) and the expansion of larch to the tundra (for 3-10 in per year) and to areas relatively poorly protected from wind due to topographic features (elevation, azimuth, and slope). It has also been shown that the radial tree increment correlates with summer temperatures (r = 0.65, tau = 0.39) and the amounts of precipitation in summer (r = -0.51, tau = 0-41) and winter (r = -0.70, tau = -0.48), decreases with an increase in the closeness of forest canopy (r = -0.52, p > 0.8; tau = -0.48, p > 0.95), and increases with an increase in the depth of soil thawing (r = 0.63, p > 0.9; tau = 0.46, p > 0.9). The density of undergrowth depends on temperatures in winter(tau = 0.53, p > 0.8) and summer (r = 0.98, p > 0.99, tau = 0.9, p > 0.99) and the date of the onset of the growing period (r = -0.60, p > 0.99; T = -0.4, p > 0.99) and negatively correlates with the amount of precipitation in summer (r = -0.56, p > 0.99, T = -0.38, p > 0.99). C1 Russian Acad Sci, Siberian Div, Sukachev Inst Forest, Krasnoyarsk 660036, Russia. NASA, Goddard Space Flight Ctr, Washington, DC 20546 USA. RP Kharuk, VI (reprint author), Russian Acad Sci, Siberian Div, Sukachev Inst Forest, Krasnoyarsk 660036, Russia. EM kharuk@ksc.krasn.ru; jon.ranson@nasa.gov RI Ranson, Kenneth/G-2446-2012; Im, Sergei/J-2736-2016 OI Ranson, Kenneth/0000-0003-3806-7270; Im, Sergei/0000-0002-5794-7938 NR 17 TC 31 Z9 32 U1 0 U2 10 PU MAIK NAUKA/INTERPERIODICA/SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013-1578 USA SN 1067-4136 J9 RUSS J ECOL+ JI Russ. J. Ecol. PD SEP-OCT PY 2006 VL 37 IS 5 BP 291 EP 298 DI 10.1134/S1067413606050018 PG 8 WC Ecology SC Environmental Sciences & Ecology GA 086VJ UT WOS:000240700800001 ER PT J AU Hansen, JE AF Hansen, James E. TI Can we still avoid dangerous human-made climate change? SO SOCIAL RESEARCH LA English DT Article; Proceedings Paper CT Fall Annual Meeting of the American-Geophysical-Union CY 2005 CL San Francisco, CA SP Amer Geophys Union C1 NASA, Goddard Inst Space Studies, Greenbelt, MD 20771 USA. NASA, Goddard Space Flight Ctr, Earth Sun Explorat Div, Greenbelt, MD 20771 USA. Columbia Univ, Earth Inst, New York, NY 10027 USA. RP Hansen, JE (reprint author), NASA, Goddard Inst Space Studies, Greenbelt, MD 20771 USA. NR 11 TC 6 Z9 6 U1 0 U2 3 PU NEW SCHOOL UNIV PI NEW YORK PA GRADUATE FACULTY, 65 5TH AVE, RM 354, NEW YORK, NY 10003 USA SN 0037-783X J9 SOC RES JI Soc. Res. PD FAL PY 2006 VL 73 IS 3 BP 949 EP 971 PG 23 WC Social Sciences, Interdisciplinary SC Social Sciences - Other Topics GA 153YF UT WOS:000245473300017 ER PT J AU Metcalf, TR Leka, KD Barnes, G Lites, BW Georgoulis, MK Pevtsov, AA Balasubramaniam, KS Gary, GA Jing, J Li, J Liu, Y Wang, HN Abramenko, V Yurchyshyn, V Moon, YJ AF Metcalf, Thomas R. Leka, K. D. Barnes, Graham Lites, Bruce W. Georgoulis, Manolis K. Pevtsov, A. A. Balasubramaniam, K. S. Gary, G. Allen Jing, Ju Li, Jing Liu, Y. Wang, H. N. Abramenko, Valentyna Yurchyshyn, Vasyl Moon, Y. -J. TI An overview of existing algorithms for resolving the 180 degrees ambiguity in vector magnetic fields: Quantitative tests with synthetic data SO SOLAR PHYSICS LA English DT Article ID SOLAR ACTIVE REGIONS; FORCE-FREE; PHYSICAL-PROPERTIES; MAGNETOGRAPH DATA; MISMA HYPOTHESIS; ELECTRIC-CURRENT; CONSTANT ALPHA; PHOTOSPHERE; EXTRAPOLATION; MORPHOLOGY AB We report here on the present state-of-the-art in algorithms used for resolving the 180 degrees ambiguity in solar vector magnetic field measurements. With present observations and techniques, some assumption must be made about the solar magnetic field in order to resolve this ambiguity. Our focus is the application of numerous existing algorithms to test data for which the correct answer is known. In this context, we compare the algorithms quantitatively and seek to understand where each succeeds, where it fails, and why. We have considered five basic approaches: comparing the observed field to a reference field or direction, minimizing the vertical gradient of the magnetic pressure, minimizing the vertical current density, minimizing some approximation to the total current density, and minimizing some approximation to the field's divergence. Of the automated methods requiring no human intervention, those which minimize the square of the vertical current density in conjunction with an approximation for the vanishing divergence of the magnetic field show the most promise. C1 NW Res Associates, Colorado Res Associates Div, Boulder, CO 80301 USA. Natl Ctr Atmospher Res, High Altitude Observ, Boulder, CO 80307 USA. Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA. Natl Solar Observ, Sunspot, NM 88349 USA. NASA, George C Marshall Space Flight Ctr, NSSTC, Huntsville, AL 35812 USA. New Jersey Inst Technol, Ctr Solar Terr Res, Newark, NJ 07102 USA. Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. Stanford Univ, Stanford, CA 94305 USA. Chinese Acad Sci, Natl Astron Observ, Beijing 100012, Peoples R China. New Jersey Inst Technol, Big Bear Solar Observ, Big Bear City, CA 92314 USA. Korea Astron & Space Sci Inst, Taejon 305348, South Korea. RP Metcalf, TR (reprint author), NW Res Associates, Colorado Res Associates Div, 3380 Mitchell Ln, Boulder, CO 80301 USA. EM metcalf@cora.nwra.com RI Moon, Yong-Jae/E-1711-2013 NR 43 TC 168 Z9 168 U1 0 U2 6 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0038-0938 J9 SOL PHYS JI Sol. Phys. PD SEP PY 2006 VL 237 IS 2 BP 267 EP 296 DI 10.1007/s11207-006-0170-x PG 30 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 085PM UT WOS:000240616000003 ER PT J AU Basilevsky, AT Rodin, AV Raitala, J Neukum, G Werner, S Kozyrev, AS Sanin, AB Mitrofanov, IG Head, JW Boynton, W Saunders, RS AF Basilevsky, A. T. Rodin, A. V. Raitala, J. Neukum, G. Werner, S. Kozyrev, A. S. Sanin, A. B. Mitrofanov, I. G. Head, J. W. Boynton, W. Saunders, R. S. TI Search for causes of the low epithermal neutron flux anomaly in the Arabia Terra region (Mars) SO SOLAR SYSTEM RESEARCH LA English DT Article ID THERMAL EMISSION SPECTROMETER; RAREFIED TURBULENT ATMOSPHERES; MERIDIANI-PLANUM; MARTIAN ATMOSPHERE; CLOUD MICROPHYSICS; HYDROUS MINERALS; SUBSURFACE ICE; MOMENT METHOD; NEAR-SURFACE; WATER-VAPOR AB A geologic analysis of 274 images acquired by the high-resolution MOC camera onboard the Mars Global Surveyor spacecraft within the Arabia Terra low neutron flux anomaly (which is indicative of an anomalously high abundance of hydrogen: up to 16 wt % of the equivalent amount of water) was performed. Correlation between the enhanced abundance of equivalent water with the presence of dust on the surface was found. Since dust plays a key role in condensation of water from the atmosphere, we suppose that the anomalies could result from the retention of atmospheric moisture. To analyze this suggestion, we performed a theoretical modeling that allowed us to map the planetary-scale distributions of several meteorological parameters responsible for the atmospheric moisture condensation. Two antipodal regions coinciding rather well with the Arabia Terra anomaly and the geographically antipodal anomaly southwest of Olympus Mons were found in the maps. This suggests that the anomalies are rather recent than ancient formations. They were probably formed by a sink of moisture from the atmosphere in the areas where present meteorological conditions support this sink. Geological parameters, primarily the presence of dust, only promote this process. We cannot exclude the possibility that the Martian cryosphere, rather than the atmosphere, supplied the studied anomalies with moisture during their formation: the thermodynamic conditions in the anomaly areas could block the moisture flux from the Martian interior in the upper regolith layer. The moisture coming from the atmosphere or from the interior is likely held as chemically bound water entering into the structure of water-bearing minerals (probably, hydrated magnesium sulfates) directly from the vapor; or the moisture precipitates as frost, penetrates into microtissures, and then is bound in minerals. Probably, another geologic factor-the magnesium sulfate abundance-works in the Arabia Terra anomaly. C1 Russian Acad Sci, VI Vernadskii Inst Geochem & Analyt Chem, Moscow 119991, Russia. Russian Acad Sci, Space Res Inst, Moscow 117997, Russia. Univ Oulu, Dept Astron, Oulu, Finland. Free Univ Berlin, Inst Geosci, D-12045 Berlin, Germany. Brown Univ, Dept Geol Sci, Providence, RI 02912 USA. Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Basilevsky, AT (reprint author), Russian Acad Sci, VI Vernadskii Inst Geochem & Analyt Chem, Ul Kosygina 19, Moscow 119991, Russia. RI Werner, Stephanie/A-6438-2012 OI Werner, Stephanie/0000-0001-5704-0909 NR 71 TC 4 Z9 4 U1 0 U2 1 PU MAIK NAUKA/INTERPERIODICA/SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013-1578 USA SN 0038-0946 EI 1608-3423 J9 SOLAR SYST RES+ JI Solar Syst. Res. PD SEP-OCT PY 2006 VL 40 IS 5 BP 355 EP 374 DI 10.1134/S0038094606050017 PG 20 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 099CZ UT WOS:000241571400001 ER PT J AU Moyes, CD Fragoso, N Musyl, MK Brill, RW AF Moyes, Christopher D. Fragoso, Nuno Musyl, Michael K. Brill, Richard W. TI Predicting postrelease survival in large pelagic fish SO TRANSACTIONS OF THE AMERICAN FISHERIES SOCIETY LA English DT Article ID ATLANTIC BLUEFIN TUNA; GULF-OF-MEXICO; ULTRASONIC TELEMETRY; MAKAIRA-NIGRICANS; THUNNUS-THYNNUS; SHARK BYCATCH; MARLIN; MOVEMENTS; POPULATIONS; METABOLISM AB Sharks, turtles, billfish, and marine mammals are frequently caught accidentally in commercial fisheries. Although conservationists and fisheries managers encourage the release of these nontarget species, the long-term outcome of released animals is uncertain. Using blue sharks Prionace glauca, we developed a model to predict the long-term survival of released animals based on analysis of small blood samples. About 5% of the sharks were landed in obviously poor condition (lethargic and unresponsive to handling); these moribund sharks were sampled and euthanized. A subset of the remaining sharks was sampled and tagged with pop-up satellite archival tags (PSATs). Each of the PSAT's that reported data (I I tags) showed that the sharks roamed at sea for at least 3 weeks postrelease. Five variables differentiated moribund sharks from survivors: plasma Mg2+ (moribund, 1.57 +/- 0.08 mM; survivor, 0.98 +/- 0.05 mM; P < 0.00001), plasma lactate (moribund, 27.7 +/- 4.1 mM; survivor, 5.80 +/- 2.96 mM; P < 0.001), erythrocyte heat shock protein 70 (Hsp70) mRNA (relative levels: moribund, 3.96 +/- 0.53; survivor, 1.00 +/- 0.29; P < 0.005), plasma Ca2+ (moribund, 3.70 +/- 0.14 mM; survivor, 3.13 +/- 0.11; P < 0.005), and plasma K, (moribund, 7.01 +/- 0.66 mM; survivor, 5.12 +/- 0.44 mM; P < 0.05). These analyses were used to develop logistic regression models that could "predict" the long-term survival of captured sharks, including a larger group of sharks that we sampled but did not tag. The best logistic model, which incorporated Mg2+ and lactate, successfully categorized 95% of fish of known outcome (19 of 20). These analyses suggest that sharks landed in an apparently healthy condition are likely to survive long term if released (95% survival based on biochemical analyses; 100% based on PSATs). C1 Queens Univ, Dept Biol, Kingston, ON K7L 3N6, Canada. Univ Hawaii, NOAA, Joint Inst Marine & Atmospher Res, Pelag Fisheries Res Program, Honolulu, HI 96814 USA. Virginia Inst Marine Sci, Natl Marine Fisheries Serv, Cooperat Marine Educ & Res Program, Gloucester Point, VA 23062 USA. RP Moyes, CD (reprint author), Queens Univ, Dept Biol, Kingston, ON K7L 3N6, Canada. EM moyesc@biology.queensu.ca NR 34 TC 97 Z9 100 U1 0 U2 21 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 SEP PY 2006 VL 135 IS 5 BP 1389 EP 1397 DI 10.1577/T05-224.1 PG 9 WC Fisheries SC Fisheries GA 101DF UT WOS:000241718400021 ER PT J AU DellaCorte, C AF DellaCorte, Christopher TI Pass the torch - not the buck 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 cdellacorte@stle.org NR 0 TC 1 Z9 1 U1 0 U2 0 PU SOC TRIBOLOGISTS & LUBRICATION ENGINEERS PI PARK RIDGE PA 840 BUSSE HIGHWAY, PARK RIDGE, IL 60068 USA SN 0024-7154 J9 TRIBOL LUBR TECHNOL JI Tribol. Lubr. Technol. PD SEP PY 2006 VL 62 IS 9 BP 6 EP 6 PG 1 WC Engineering, Mechanical SC Engineering GA 089OJ UT WOS:000240889800002 ER PT J AU Mansour, K Qiu, Y Hill, CJ Soibel, A Yang, RQ AF Mansour, K. Qiu, Y. Hill, C. J. Soibel, A. Yang, R. Q. TI Mid-infrared interband cascade lasers at thermoelectric cooler temperatures SO ELECTRONICS LETTERS LA English DT Article ID CONTINUOUS-WAVE OPERATION; ROOM-TEMPERATURE AB Continuous-wave operation of a mid-infrared (similar to 3.3 mu m) interband cascade laser has been demonstrated at temperatures up to 264 K. The laser has also been operated continuously with a thermoelectric cooler near 260 K for more than 1900 h without observable degradation. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Mansour, K (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM Rui.Q.Yang@JPL.nasa.gov RI Soibel, Alexander/A-1313-2007 NR 10 TC 65 Z9 66 U1 0 U2 13 PU INSTITUTION ENGINEERING TECHNOLOGY-IET PI HERTFORD PA MICHAEL FARADAY HOUSE SIX HILLS WAY STEVENAGE, HERTFORD SG1 2AY, ENGLAND SN 0013-5194 J9 ELECTRON LETT JI Electron. Lett. PD AUG 31 PY 2006 VL 42 IS 18 BP 1034 EP 1036 DI 10.1049/el:20062442 PG 3 WC Engineering, Electrical & Electronic SC Engineering GA 091GZ UT WOS:000241016400016 ER PT J AU Campana, S Mangano, V Blustin, AJ Brown, P Burrows, DN Chincarini, G Cummings, JR Cusumano, G Della Valle, M Malesani, D Meszaros, P Nousek, JA Page, M Sakamoto, T Waxman, E Zhang, B Dai, ZG Gehrels, N Immler, S Marshall, FE Mason, KO Moretti, A O'Brien, PT Osborne, JP Page, KL Romano, P Roming, PWA Tagliaferri, G Cominsky, LR Giommi, P Godet, O Kennea, JA Krimm, H Angelini, L Barthelmy, SD Boyd, PT Palmer, DM Wells, AA White, NE AF Campana, S. Mangano, V. Blustin, A. J. Brown, P. Burrows, D. N. Chincarini, G. Cummings, J. R. Cusumano, G. Della Valle, M. Malesani, D. Meszaros, P. Nousek, J. A. Page, M. Sakamoto, T. Waxman, E. Zhang, B. Dai, Z. G. Gehrels, N. Immler, S. Marshall, F. E. Mason, K. O. Moretti, A. O'Brien, P. T. Osborne, J. P. Page, K. L. Romano, P. Roming, P. W. A. Tagliaferri, G. Cominsky, L. R. Giommi, P. Godet, O. Kennea, J. A. Krimm, H. Angelini, L. Barthelmy, S. D. Boyd, P. T. Palmer, D. M. Wells, A. A. White, N. E. TI The association of GRB 060218 with a supernova and the evolution of the shock wave SO NATURE LA English DT Article ID GAMMA-RAY BURSTS; 25 APRIL 1998; RADIO-EMISSION; SN 1998BW; TELESCOPE; MISSION AB Although the link between long gamma-ray bursts (GRBs) and supernovae has been established(1-4), hitherto there have been no observations of the beginning of a supernova explosion and its intimate link to a GRB. In particular, we do not know how the jet that defines a gamma-ray burst emerges from the star's surface, nor how a GRB progenitor explodes. Here we report observations of the relatively nearby GRB 060218 (ref. 5) and its connection to supernova SN 2006aj ( ref. 6). In addition to the classical non-thermal emission, GRB 060218 shows a thermal component in its X-ray spectrum, which cools and shifts into the optical/ ultraviolet band as time passes. We interpret these features as arising from the break-out of a shock wave driven by a mildly relativistic shell into the dense wind surrounding the progenitor(7). We have caught a supernova in the act of exploding, directly observing the shock break-out, which indicates that the GRB progenitor was a Wolf Rayet star. C1 Osserv Astron Brera, INAF, I-23807 Merate, LC, Italy. Ist Astrofis Spaziale & Fis Cosm Palermo, INAF, I-90146 Palermo, Italy. UCL, Mullard Space Sci Lab, Dorking RH5 6NT, Surrey, England. Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. Univ Milano Bicocca, I-20126 Milan, Italy. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. CNR, Washington, DC 20418 USA. Osserv Astrofis Arcetri, INAF, I-50125 Florence, Italy. Univ Calif Santa Barbara, Kavli Inst Theoret Phys, Santa Barbara, CA 93106 USA. SISSA, ISAS, I-34014 Trieste, Italy. Penn State Univ, Dept Phys, University Pk, PA 16802 USA. Weizmann Inst Sci, Fac Phys, IL-76100 Rehovot, Israel. Univ Nevada, Dept Phys, Las Vegas, NV 89154 USA. Nanjing Univ, Dept Astron, Nanjing 210093, Peoples R China. PPARC, Swindon SN2 1SZ, Wilts, England. Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England. Sonoma State Univ, Dept Phys & Astron, Rohnert Pk, CA 94928 USA. ASI Sci Data Ctr, I-00044 Frascati, Roma, Italy. Univ Space Res Assoc, Columbia, MD 21044 USA. Los Alamos Natl Lab, Los Alamos, NM 87545 USA. RP Campana, S (reprint author), Osserv Astron Brera, INAF, Via E Bianchi 46, I-23807 Merate, LC, Italy. EM sergio.campana@brera.inaf.it RI White, Nicholas/B-6428-2012; Barthelmy, Scott/D-2943-2012; Boyd, Patricia/D-3274-2012; Gehrels, Neil/D-2971-2012; WAXMAN, ELI/K-1557-2012; OI White, Nicholas/0000-0003-3853-3462; giommi, paolo/0000-0002-2265-5003; Cusumano, Giancarlo/0000-0002-8151-1990; moretti, alberto/0000-0002-9770-0315; Della Valle, Massimo/0000-0003-3142-5020; Tagliaferri, Gianpiero/0000-0003-0121-0723 NR 28 TC 464 Z9 470 U1 2 U2 26 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 0028-0836 J9 NATURE JI Nature PD AUG 31 PY 2006 VL 442 IS 7106 BP 1008 EP 1010 DI 10.1038/nature04892 PG 3 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 078YF UT WOS:000240142000041 PM 16943830 ER PT J AU Pian, E Mazzali, PA Masetti, N Ferrero, P Klose, S Palazzi, E Ramirez-Ruiz, E Woosley, SE Kouveliotou, C Deng, J Filippenko, AV Foley, RJ Fynbo, JPU Kann, DA Li, W Hjorth, J Nomoto, K Patat, F Sauer, DN Sollerman, J Vreeswijk, PM Guenther, EW Levan, A O'Brien, P Tanvir, NR Wijers, RAMJ Dumas, C Hainaut, O Wong, DS Baade, D Wang, L Amati, L Cappellaro, E Castro-Tirado, AJ Ellison, S Frontera, F Fruchter, AS Greiner, J Kawabata, K Ledoux, C Maeda, K Moller, P Nicastro, L Rol, E Starling, R AF Pian, E. Mazzali, P. A. Masetti, N. Ferrero, P. Klose, S. Palazzi, E. Ramirez-Ruiz, E. Woosley, S. E. Kouveliotou, C. Deng, J. Filippenko, A. V. Foley, R. J. Fynbo, J. P. U. Kann, D. A. Li, W. Hjorth, J. Nomoto, K. Patat, F. Sauer, D. N. Sollerman, J. Vreeswijk, P. M. Guenther, E. W. Levan, A. O'Brien, P. Tanvir, N. R. Wijers, R. A. M. J. Dumas, C. Hainaut, O. Wong, D. S. Baade, D. Wang, L. Amati, L. Cappellaro, E. Castro-Tirado, A. J. Ellison, S. Frontera, F. Fruchter, A. S. Greiner, J. Kawabata, K. Ledoux, C. Maeda, K. Moller, P. Nicastro, L. Rol, E. Starling, R. TI An optical supernova associated with the X-ray flash XRF 060218 SO NATURE LA English DT Article ID LOW-LUMINOSITY; LIGHT-CURVE; BURST; AFTERGLOW; MODELS; GRB-030329; GRB-031203; DISCOVERY; SN-2006AJ; EMISSION AB Long-duration gamma-ray bursts (GRBs) are associated with type Ic supernovae(1) that are more luminous than average(2-5) and that eject material at very high velocities. Less-luminous supernovae were not hitherto known to be associated with GRBs, and therefore GRB - supernovae were thought to be rare events(6). Whether X-ray flashes - analogues of GRBs, but with lower luminosities and fewer gamma-rays - can also be associated with supernovae, and whether they are intrinsically 'weak' events or typical GRBs viewed off the axis of the burst(7), is unclear. Here we report the optical discovery and follow-up observations of the type Ic supernova SN 2006aj associated with X-ray flash XRF 060218. Supernova 2006aj is intrinsically less luminous than the GRB - supernovae, but more luminous than many supernovae not accompanied by a GRB. The ejecta velocities derived from our spectra are intermediate between these two groups, which is consistent with the weakness of both the GRB output(8) and the supernova radio flux(9). Our data, combined with radio and X-ray observations(8-10), suggest that XRF 060218 is an intrinsically weak and soft event, rather than a classical GRB observed off-axis. This extends the GRB - supernova connection to X-ray flashes and fainter supernovae, implying a common origin. Events such as XRF 060218 are probably more numerous than GRB - supernovae. C1 Trieste Astron Observ, Ist Nazl Astrofis, I-34131 Trieste, Italy. Univ Calif Santa Barbara, Kavli Inst Theoret Phys, Santa Barbara, CA 93106 USA. Max Planck Inst Astrophys, D-85748 Garching, Germany. Univ Tokyo, Sch Sci, Dept Astron, Bunkyo Ku, Tokyo 1130033, Japan. Univ Tokyo, Sch Sci, Res Ctr Early Universe, Bunkyo Ku, Tokyo 1130033, Japan. IASF, Ist Nazl Astrofis, I-40129 Bologna, Italy. Thuringer Landessternwarte Tautenburg, D-07778 Tautenburg, Germany. Inst Adv Study, Princeton, NJ 08540 USA. Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA. NASA, MSFC, NSSTC, Huntsville, AL 35805 USA. Chinese Acad Sci, Natl Astron Observ, Beijing 100012, Peoples R China. Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. Univ Copenhagen, Niels Bohr Inst, Dark Cosmol Ctr, DK-2100 Copenhagen O, Denmark. European So Observ, D-85748 Garching, Germany. Stockholm Univ, Dept Astron, S-10691 Stockholm, Sweden. Univ Chile, Dept Astron, Santiago, Chile. European So Observ, Santiago 19, Chile. Univ Hertfordshire, Ctr Astrophys Res, Hatfield AL10 9AB, Herts, England. Univ Leicester, Dept Phys & Astron, Xray & Observat Astron Grp, Leicester LE1 7RH, Leics, England. Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1098 SJ Amsterdam, Netherlands. Univ Calif Berkeley, Lawrence Berkeley Lab, Berkeley, CA 94720 USA. Chinese Acad Sci, Purple Mt Observ, Nanjing 210008, Jiangsu, Peoples R China. Padova Astron Observ, Ist Nazl Astrofis, I-35122 Padua, Italy. CSIC, IAA, E-18080 Granada, Spain. Univ Victoria, Dept Phys & Astron, Victoria, BC V8P 1A1, Canada. Univ Ferrara, Dept Phys, I-44100 Ferrara, Italy. Space Telescope Sci Inst, Baltimore, MD 21218 USA. Max Planck Inst Extraterr Phys, D-85741 Garching, Germany. Hiroshima Univ, Hiroshima Astrophys Sci Ctr, Hiroshima 7398526, Japan. Univ Tokyo, Coll Arts & Sci, Dept Earth Sci & Astron, Meguro Ku, Tokyo 1538902, Japan. RP Pian, E (reprint author), Trieste Astron Observ, Ist Nazl Astrofis, Via GB Tiepolo 11, I-34131 Trieste, Italy. EM pian@oats.inaf.it RI Fynbo, Johan/L-8496-2014; Hjorth, Jens/M-5787-2014; Sauer, Daniel/A-3033-2012; Palazzi, Eliana/N-4746-2015; Amati, Lorenzo/N-5586-2015; OI Masetti, Nicola/0000-0001-9487-7740; Fynbo, Johan/0000-0002-8149-8298; Hjorth, Jens/0000-0002-4571-2306; Sauer, Daniel/0000-0002-0317-5063; Amati, Lorenzo/0000-0001-5355-7388; Castro-Tirado, A. J./0000-0003-2999-3563; Wijers, Ralph/0000-0002-3101-1808; Palazzi, Eliana/0000-0002-8691-7666; Patat, Ferdinando/0000-0002-0537-3573; Sollerman, Jesper/0000-0003-1546-6615 NR 30 TC 336 Z9 339 U1 1 U2 18 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 0028-0836 J9 NATURE JI Nature PD AUG 31 PY 2006 VL 442 IS 7106 BP 1011 EP 1013 DI 10.1038/nature05082 PG 3 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 078YF UT WOS:000240142000042 PM 16943831 ER PT J AU Soderberg, AM Kulkarni, SR Nakar, E Berger, E Cameron, PB Fox, DB Frail, D Gal-Yam, A Sari, R Cenko, SB Kasliwal, M Chevalier, RA Piran, T Price, PA Schmidt, BP Pooley, G Moon, DS Penprase, BE Ofek, E Rau, A Gehrels, N Nousek, JA Burrows, DN Persson, SE McCarthy, PJ AF Soderberg, A. M. Kulkarni, S. R. Nakar, E. Berger, E. Cameron, P. B. Fox, D. B. Frail, D. Gal-Yam, A. Sari, R. Cenko, S. B. Kasliwal, M. Chevalier, R. A. Piran, T. Price, P. A. Schmidt, B. P. Pooley, G. Moon, D. -S. Penprase, B. E. Ofek, E. Rau, A. Gehrels, N. Nousek, J. A. Burrows, D. N. Persson, S. E. McCarthy, P. J. TI Relativistic ejecta from X-ray flash XRF 060218 and the rate of cosmic explosions SO NATURE LA English DT Article ID 25 APRIL 1998; UNUSUAL SUPERNOVA; BURST; PROGENITORS; GRB-980425; LUMINOSITY; EMISSION; PULSAR AB Over the past decade, long-duration gamma-ray bursts (GRBs) - including the subclass of X-ray flashes (XRFs) - have been revealed(1-3) to be a rare variety of type Ibc supernova. Although all these events result from the death of massive stars, the electromagnetic luminosities of GRBs and XRFs exceed those of ordinary type Ibc supernovae by many orders of magnitude. The essential physical process that causes a dying star to produce a GRB or XRF, and not just a supernova, is still unknown. Here we report radio and X-ray observations of XRF 060218 ( associated(4) with supernova SN 2006aj), the second-nearest(5,6) GRB identified until now. We show that this event is a hundred times less energetic but ten times more common than cosmological GRBs. Moreover, it is distinguished from ordinary type Ibc supernovae by the presence of 10(48) erg coupled to mildly relativistic ejecta, along with a central engine ( an accretion-fed, rapidly rotating compact source) that produces X-rays for weeks after the explosion. This suggests that the production of relativistic ejecta is the key physical distinction between GRBs or XRFs and ordinary supernovae, while the nature of the central engine ( black hole or magnetar) may distinguish typical bursts from low-luminosity, spherical events like XRF 060218. C1 CALTECH, Caltech Opt Observ 105 24, Pasadena, CA 91125 USA. CALTECH, Space Radiat Lab 220 47, Pasadena, CA 91125 USA. Carnegie Observ, Pasadena, CA 91101 USA. Penn State Univ, Dept Astron, University Pk, PA 16802 USA. Natl Radio Astron Observ, Socorro, NM 87801 USA. Univ Virginia, Dept Astron, Charlottesville, VA 22903 USA. Hebrew Univ Jerusalem, Racah Inst Phys, IL-91904 Jerusalem, Israel. Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. ANU, Mt Stromlo Observ, RSAA, Weston, ACT 2611, Australia. Univ Cambridge, Cavendish Lab, Mullard Radio Astron Observ, Cambridge CB3 0HE, England. Pomona Coll, Dept Phys & Astron, Claremont, CA 91711 USA. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Soderberg, AM (reprint author), CALTECH, Caltech Opt Observ 105 24, Pasadena, CA 91125 USA. EM ams@astro.caltech.edu RI Gehrels, Neil/D-2971-2012; OI Schmidt, Brian/0000-0001-6589-1287; Schmidt, Brian/0000-0002-8538-9195 NR 30 TC 297 Z9 301 U1 3 U2 14 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 0028-0836 J9 NATURE JI Nature PD AUG 31 PY 2006 VL 442 IS 7106 BP 1014 EP 1017 DI 10.1038/nature05087 PG 4 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 078YF UT WOS:000240142000043 PM 16943832 ER PT J AU Behrenfeld, MJ Worthington, K Sherrell, RM Chavez, FP Strutton, P McPhaden, M Shea, DM AF Behrenfeld, Michael J. Worthington, Kirby Sherrell, Robert M. Chavez, Francisco P. Strutton, Peter McPhaden, Michael Shea, Donald M. TI Controls on tropical Pacific Ocean productivity revealed through nutrient stress diagnostics SO NATURE LA English DT Article ID SYNECHOCOCCUS SP PCC7942; IRON-DEFICIENCY; PHOTOSYSTEM-II; ELECTRON-TRANSPORT; PHYTOPLANKTON BLOOM; SOUTHERN-OCEAN; EL-NINO; FERTILIZATION; CHLOROPHYLL; LIMITATION AB In situ enrichment experiments have shown that the growth of bloom-forming diatoms in the major high-nitrate low-chlorophyll (HNLC) regions of the world's oceans is limited by the availability of iron(1-3). Yet even the largest of these manipulative experiments represents only a small fraction of an ocean basin, and the responses observed are strongly influenced by the proliferation of rare species rather than the growth of naturally dominant populations(4,5). Here we link unique fluorescence attributes of phytoplankton to specific physiological responses to nutrient stress, and use these relationships to evaluate the factors that constrain phytoplankton growth in the tropical Pacific Ocean on an unprecedented spatial scale. On the basis of fluorescence measurements taken over 12 years, we delineate three major ecophysiological regimes in this region. We find that iron has a key function in regulating phytoplankton growth in both HNLC and oligotrophic waters near the Equator and further south, whereas nitrogen and zooplankton grazing are the primary factors that regulate biomass production in the north. Application of our findings to the interpretation of satellite chlorophyll fields shows that productivity in the tropical Pacific basin may be 1.2 - 2.5 Pg C yr(-1) lower than previous estimates have suggested, a difference that is comparable to the global change in ocean production that accompanied the largest El Nino to La Nina transition on record(6). C1 Oregon State Univ, Dept Bot & Plant Pathol, Corvallis, OR 97331 USA. NASA, Sci Applicat Int Corp, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Rutgers State Univ, Inst Marine & Coastal Sci, New Brunswick, NJ 08901 USA. Rutgers State Univ, Dept Geol Sci, New Brunswick, NJ 08901 USA. Monterey Bay Aquarium Res Inst, Moss Landing, CA 95039 USA. Oregon State Univ, Coll Ocean & Atmospher Sci, Corvallis, OR 97331 USA. NOAA, Pacific Marine Environm Lab, Seattle, WA 98115 USA. RP Behrenfeld, MJ (reprint author), Oregon State Univ, Dept Bot & Plant Pathol, Cordley Hall 2082, Corvallis, OR 97331 USA. EM mjb@science.oregonstate.edu RI Strutton, Peter/C-4466-2011; McPhaden, Michael/D-9799-2016 OI Strutton, Peter/0000-0002-2395-9471; NR 29 TC 125 Z9 136 U1 8 U2 58 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 0028-0836 J9 NATURE JI Nature PD AUG 31 PY 2006 VL 442 IS 7106 BP 1025 EP 1028 DI 10.1038/nature05083 PG 4 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 078YF UT WOS:000240142000046 PM 16943835 ER PT J AU Hoogenboom, T Srnrekar, SE AF Hoogenboom, Trudi Srnrekar, Suzanne E. TI Elastic thickness estimates for the northern lowlands of Mars SO EARTH AND PLANETARY SCIENCE LETTERS LA English DT Article DE Mars; elastic thickness; northern lowlands; admittance ID MARTIAN HEMISPHERIC DICHOTOMY; CONTINENTAL LITHOSPHERE; ISOSTATIC COMPENSATION; CRUSTAL DICHOTOMY; MANTLE CONVECTION; GRAVITY; TOPOGRAPHY; EVOLUTION; BASINS; MODELS AB The northern lowlands cover approximately one-third of Mars' surface and are a fundamental part of the geologic evolution of Mars. We examine the admittance signature, the ratio of gravity to topography data in the spectral domain, for four regions in the northern lowlands that are both well resolved in the gravity data and have well constrained lithospheric parameters. These regions also have topographic power spectra similar to many highlands regions. A Cartesian multitaper method is used to calculate admittance. We compare the observed admittance signatures to those predicted from models of lithospheric flexure. On the basis of these comparisons, we estimate the thickness of the Martian elastic lithosphere (T(e)) required to support the observed topographic load since the time of loading. We use both top and bottom loading models to derive values of elastic thickness and crustal thickness or apparent depth of compensation although all four regions are best fit by bottom loading models. We obtain best fit elastic thickness estimates between 10 and 25 km with an acceptable error range of 0 to 45 km. These low elastic thickness estimates are consistent with the formation in the Noachian, when heat flow was high. The consistency in T(e) estimates between the Noachian highlands and lowlands basement suggests that both regions of the crust formed at similar times. The paucity of crustal magnetization in the lowlands is thus more likely a result of demagnetization than formation following shut down of the dynamo. (c) 2006 Elsevier B.V. All rights reserved. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Hoogenboom, T (reprint author), ExxonMobil Explorat Co, Technol Geophys Operat, CORP GP8 688B, Houston, TX USA. EM Trudi.M.Hoogenboom@exxonmobil.com NR 45 TC 18 Z9 18 U1 0 U2 0 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 AUG 30 PY 2006 VL 248 IS 3-4 BP 830 EP 839 DI 10.1016/j.epsl.2006.06.035 PG 10 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 085KG UT WOS:000240602400018 ER PT J AU Barnes, JW Brown, RH Radebaugh, J Buratti, BJ Sotin, C Le Mouelic, S Rodriguez, S Turtle, EP Perry, J Clark, R Baines, KH Nicholson, PD AF Barnes, Jason W. Brown, Robert H. Radebaugh, Jani Buratti, Bonnie J. Sotin, Christophe Le Mouelic, Stephane Rodriguez, Sebastien Turtle, Elizabeth P. Perry, Jason Clark, Roger Baines, Kevin H. Nicholson, Phillip D. TI Cassini observations of flow-like features in western Tui Regio, Titan SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID ACOUSTIC FLUIDIZATION; SURFACE; MOBILITY; WINDS AB A large (> 3 x 10(4) km(2)), lobate, 5-mu m-bright region seen by Cassini on Titan's leading equatorial region is best explained as a flow field. We discuss observations from the Visual and Infrared Mapping Spectrometer and Imaging Science Subsystem of the feature and present a map of the field. We establish relative ages of flow features and discuss possible formation mechanisms and the implications of this finding for the evolution of Titan's surface. C1 Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. Univ Nantes, UMR CNRS, Lab Planetol & Geodynam, F-44322 Nantes, France. US Geol Survey, Denver, CO 80225 USA. Cornell Univ, Dept Astron, Ithaca, NY 14853 USA. RP Barnes, JW (reprint author), Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA. EM jbarnes@lpl.arizona.edu RI Barnes, Jason/B-1284-2009; Turtle, Elizabeth/K-8673-2012; Rodriguez, Sebastien/H-5902-2016 OI Barnes, Jason/0000-0002-7755-3530; Turtle, Elizabeth/0000-0003-1423-5751; Rodriguez, Sebastien/0000-0003-1219-0641 NR 17 TC 45 Z9 46 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 AUG 30 PY 2006 VL 33 IS 16 AR L16204 DI 10.1029/2006GL026843 PG 5 WC Geosciences, Multidisciplinary SC Geology GA 081QA UT WOS:000240330900005 ER PT J AU de Goncalves, LGG Shuttleworth, WJ Nijssen, B Burke, EJ Marengo, JA Chou, SC Houser, P Toll, DL AF Gustavo Goncalves de Goncalves, L. Shuttleworth, W. James Nijssen, Bart Burke, Eleanor J. Marengo, Jose A. Chou, Sin Chan Houser, Paul Toll, David L. TI Evaluation of model-derived and remotely sensed precipitation products for continental South America SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID GENERAL-CIRCULATION MODELS; LEVEL JET EAST; GLOBAL PRECIPITATION; INTERANNUAL VARIABILITY; UNITED-STATES; ETA-MODEL; CLIMATOLOGY; RAINFALL; TRMM; ATMOSPHERE AB [ 1] This paper investigates the reliability of some of the more important remotely sensed daily precipitation products available for South America as a precursor to the possible implementation of a South America Land Data Assimilation System. Precipitation data fields calculated as 6 hour predictions by the CPTEC Eta model and three different satellite-derived estimates of precipitation ( Precipitation Estimation from Remotely Sensed Information using Artificial Neural Networks (PERSIANN), National Environmental Satellite, Data and Information Service (NESDIS), and Tropical Rainfall Measuring Mission (TRMM)) are compared with the available observations of daily total rainfall across South America. To make this comparison, the threat score, fractional-covered area, and relative volumetric bias of the model-calculated and remotely sensed estimates are computed for the year 2000. The results show that the Eta model-calculated data and the NESDIS product capture the area without precipitation within the domain reasonably well, while the TRMM and PERSIANN products tend to underestimate the area without precipitation and to heavily overestimate the area with a small amount of precipitation. In terms of precipitation amount the NESDIS product significantly overestimates and the TRMM product significantly underestimates precipitation, while the Eta model-calculated data and PERSIANN product broadly match the domain average observations. However, both tend to bias the zonal location of precipitation more heavily toward the equator than the observations. In general, the Eta model-calculated data outperform the several remotely sensed data products currently available and evaluated in the present study. C1 Univ Arizona, Dept Hydrol & Water Resources, Tucson, AZ 85721 USA. Met Off, Hadley Ctr Climate Predict & Res, Exeter EX1 3PB, Devon, England. Inst Nacl Pesquisas Espaciais, Ctr Previsao Tempo & Estudos Climat, BR-12630000 Sao Paulo, Brazil. George Mason Univ, Ctr Res Environm & Water, Beltsville, MD 20705 USA. NASA, Goddard Space Flight Ctr, Hydrol Sci Branch, Greenbelt, MD 20771 USA. RP de Goncalves, LGG (reprint author), NASA, Goddard Space Flight Ctr, Hydrol Sci Branch, Code 614-3, Greenbelt, MD 20771 USA. EM gustavo@hsb.gsfc.nasa.gov RI de Goncalves, Luis Gustavo/G-2522-2012; Houser, Paul/J-9515-2013; Nijssen, Bart/B-1013-2012; Marengo, Jose /J-9382-2012; Chou, Sin Chan/F-6364-2012; OI Houser, Paul/0000-0002-2991-0441; Nijssen, Bart/0000-0002-4062-0322; Marengo, Jose /0000-0002-8154-2762; Chou, Sin Chan/0000-0002-8973-1808; de Goncalves, Luis Gustavo/0000-0002-1571-0916 NR 60 TC 18 Z9 18 U1 0 U2 5 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X EI 2169-8996 J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD AUG 30 PY 2006 VL 111 IS D16 AR D16113 DI 10.1029/2005JD006276 PG 13 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 081QY UT WOS:000240333300001 ER PT J AU Walker, JT Robarge, WP Wu, Y Meyers, TP AF Walker, J. T. Robarge, W. P. Wu, Y. Meyers, T. P. TI Measurement of bi-directional ammonia fluxes over soybean using the modified Bowen-ratio technique SO AGRICULTURAL AND FOREST METEOROLOGY LA English DT Article DE ammonia; dry deposition; compensation point; soybean; bi-directional flux ID ATMOSPHERIC NITROGEN DEPOSITION; DRY DEPOSITION; COMPENSATION POINT; SURFACE-EXCHANGE; GRADIENT MEASUREMENTS; NORTH-CAROLINA; UNITED-STATES; OILSEED RAPE; VEGETATED SURFACES; LOLIUM-PERENNE AB Measurements of bi-directional ammonia (NH3) exchange over a fertilized soybean canopy are presented for an 8-week period during the summer of 2002. The modified Bowen-ratio approach was used to determine fluxes from vertical NH3 and temperature gradients in combination with eddy covariance sensible heat fluxes. The measurement site is located in an area of high NH3 emissions from animal production and fertilizer use. Ambient NH3 concentrations ranged from 0.01 to 43.9 mu g m(-3) (mu = 9.4 mu g m(-3)) during the experiment. The mean flux was -12.3 ng m(-2) s(-1), indicating that the canopy was a net sink for NH3; however, emission fluxes were consistently observed during the late morning and early afternoon. Deposition rates were highest when the canopy was wet (mu = -29.9 ng m(-2) s(-1)). Modeling results suggest that uptake via the leaf cuticle was the dominant deposition process and stomatal uptake only occurred during the first few hours after sunrise when the stomatal resistance and compensation point were low. The average stomatal compensation point was high (chi(s) = 11.5 mu g NH3 m(-3)), primarily due to high daytime temperatures (mu = 29 degrees C). Measured cuticular resistances were large (median R-w = 208 s m(-1)), most likely due to very dry conditions. The average NH3 flux corresponds to a dry-to-wet deposition ratio of 0.44. Median flux error was 51%, which was dominated by uncertainty in the vertical NH3 gradient due to sequential sampling between measurement heights. (c) 2006 Elsevier B.V. All rights reserved. C1 US EPA, Natl Risk Management Res Lab, Res Triangle Pk, NC 27711 USA. N Carolina State Univ, Dept Soil Sci, Raleigh, NC 27695 USA. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Natl Ocean & Atmospher Adm, Atmospher Turbulence & Diffus Div, Oak Ridge, TN 37830 USA. RP Walker, JT (reprint author), US EPA, Natl Risk Management Res Lab, Res Triangle Pk, NC 27711 USA. EM walker.johnt@epa.gov RI Walker, John/I-8880-2014; Meyers, Tilden/C-6633-2016 OI Walker, John/0000-0001-6034-7514; NR 75 TC 48 Z9 49 U1 0 U2 16 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0168-1923 J9 AGR FOREST METEOROL JI Agric. For. Meteorol. PD AUG 29 PY 2006 VL 138 IS 1-4 BP 54 EP 68 DI 10.1016/j.agrformet.2006.03.011 PG 15 WC Agronomy; Forestry; Meteorology & Atmospheric Sciences SC Agriculture; Forestry; Meteorology & Atmospheric Sciences GA 079ZQ UT WOS:000240216800005 ER PT J AU Grant, JA Wilson, SA Ruff, SW Golombek, MP Koestler, DL AF Grant, J. A. Wilson, S. A. Ruff, S. W. Golombek, M. P. Koestler, D. L. TI Distribution of rocks on the Gusev Plains and on Husband Hill, Mars SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID SIZE-FREQUENCY DISTRIBUTIONS; SPIRIT ROVER; MAADIM-VALLIS; CRATER; DEPOSITS; BASIN; SITES AB The population of rocks larger than 15 cm in diameter was measured at 36 locations imaged by the Spirit rover over similar to 4 km of the traverse across the Gusev plains and Husband Hill in Gusev crater on Mars. The rock population observed on plains surfaces is consistent with impact fragmentation of rubbly/ fractured volcanics and reveals little evidence for modification by secondary processes or weathering. Interpretation of counts from Husband Hill suggest an influence by bedrock for rocks larger than 0.5 m across, but the distribution of smaller rocks is consistent with ejecta possessing contributions from pre-plains impact events. Results indicate plains surfaces experienced only tens of centimeters of eolian erosion/deposition since the Hesperian, whereas meters rather than tens of meters of erosion modified Husband Hill since the early Hesperian. C1 Smithsonian Inst, Natl Air & Space Museum, Ctr Earth & Planetary Sci, Washington, DC 20560 USA. Arizona State Univ, Dept Geol Sci, Tempe, AZ 85287 USA. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. E Stroudsburg Univ, Dept Comp Sci, E Stroudsburg, PA 18301 USA. RP Grant, JA (reprint author), Smithsonian Inst, Natl Air & Space Museum, Ctr Earth & Planetary Sci, 6th & Independence Ave SW, Washington, DC 20560 USA. EM grantj@si.edu NR 30 TC 21 Z9 21 U1 0 U2 0 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 EI 1944-8007 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD AUG 29 PY 2006 VL 33 IS 16 AR L16202 DI 10.1029/2006GL026964 PG 6 WC Geosciences, Multidisciplinary SC Geology GA 081PZ UT WOS:000240330800004 ER PT J AU Schwarz, JP Gao, RS Fahey, DW Thomson, DS Watts, LA Wilson, JC Reeves, JM Darbeheshti, M Baumgardner, DG Kok, GL Chung, SH Schulz, M Hendricks, J Lauer, A Karcher, B Slowik, JG Rosenlof, KH Thompson, TL Langford, AO Loewenstein, M Aikin, KC AF Schwarz, J. P. Gao, R. S. Fahey, D. W. Thomson, D. S. Watts, L. A. Wilson, J. C. Reeves, J. M. Darbeheshti, M. Baumgardner, D. G. Kok, G. L. Chung, S. H. Schulz, M. Hendricks, J. Lauer, A. Kaercher, B. Slowik, J. G. Rosenlof, K. H. Thompson, T. L. Langford, A. O. Loewenstein, M. Aikin, K. C. TI Single-particle measurements of midlatitude black carbon and light-scattering aerosols from the boundary layer to the lower stratosphere SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID ELEMENTAL CARBON; AIRCRAFT EMISSIONS; ORGANIC AEROSOL; SPECTROMETER; SIZE; SOOT; INSTRUMENT; ABSORPTION; SULFATE; SULFUR AB [ 1] A single-particle soot photometer (SP2) was flown on a NASA WB-57F high-altitude research aircraft in November 2004 from Houston, Texas. The SP2 uses laser-induced incandescence to detect individual black carbon ( BC) particles in an air sample in the mass range of similar to 3 - 300 fg ( similar to 0.15 - 0.7 mu m volume equivalent diameter). Scattered light is used to size the remaining non-BC aerosols in the range of similar to 0.17 - 0.7 mu m diameter. We present profiles of both aerosol types from the boundary layer to the lower stratosphere from two midlatitude flights. Results for total aerosol amounts in the size range detected by the SP2 are in good agreement with typical particle spectrometer measurements in the same region. All ambient incandescing particles were identified as BC because their incandescence properties matched those of laboratory-generated BC aerosol. Approximately 40% of these BC particles showed evidence of internal mixing ( e. g., coating). Throughout profiles between 5 and 18.7 km, BC particles were less than a few percent of total aerosol number, and black carbon aerosol (BCA) mass mixing ratio showed a constant gradient with altitude above 5 km. SP2 data was compared to results from the ECHAM4/MADE and LmDzT-INCA global aerosol models. The comparison will help resolve the important systematic differences in model aerosol processes that determine BCA loadings. Further intercomparisons of models and measurements as presented here will improve the accuracy of the radiative forcing contribution from BCA. C1 NOAA, Div Chem Sci, Earth Syst Res Lab, Boulder, CO 80305 USA. Univ Colorado, Cooperat Inst Res Environm Sci, Boulder, CO 80309 USA. Univ Denver, Dept Engn, Denver, CO 80208 USA. Univ Nacl Autonoma Mexico, Ctr Ciencias Atmosfera, Mexico City 04510, DF, Mexico. Droplet Measurement Technol Inc, Boulder, CO USA. Lab Sci Climat & Environm, F-91191 Gif Sur Yvette, France. DLR, Inst Phys Atmosphare, D-82234 Wessling, Germany. Boston Coll, Dept Chem, Chestnut Hill, MA 02467 USA. NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Schwarz, JP (reprint author), NOAA, Div Chem Sci, Earth Syst Res Lab, Boulder, CO 80305 USA. EM joshua.p.schwarz@noaa.gov; mdarbehe@du.edu RI Langford, Andrew/D-2323-2009; Slowik, Jay/F-4894-2011; Rosenlof, Karen/B-5652-2008; schwarz, joshua/G-4556-2013; Gao, Ru-Shan/H-7455-2013; Aikin, Kenneth/I-1973-2013; Watts, Laurel/G-4532-2013; Karcher, Bernd/D-5325-2014; Schulz, Michael/A-6930-2011; Fahey, David/G-4499-2013; Manager, CSD Publications/B-2789-2015 OI Langford, Andrew/0000-0002-2932-7061; Slowik, Jay/0000-0001-5682-850X; Rosenlof, Karen/0000-0002-0903-8270; schwarz, joshua/0000-0002-9123-2223; Watts, Laurel/0000-0002-0834-3329; Karcher, Bernd/0000-0003-0278-4980; Schulz, Michael/0000-0003-4493-4158; Fahey, David/0000-0003-1720-0634; NR 45 TC 240 Z9 251 U1 13 U2 91 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X EI 2169-8996 J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD AUG 29 PY 2006 VL 111 IS D16 AR D16207 DI 10.1029/2006JD007076 PG 15 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 081QV UT WOS:000240333000004 ER PT J AU Pulkkinen, A Viljanen, A Pirjola, R AF Pulkkinen, Antti Viljanen, Ari Pirjola, Risto TI Estimation of geomagnetically induced current levels from different input data SO SPACE WEATHER-THE INTERNATIONAL JOURNAL OF RESEARCH AND APPLICATIONS LA English DT Article ID AURORAL ELECTROJET ACTIVITY; NATURAL-GAS PIPELINE; COMPLEX-IMAGE METHOD; CURRENT SYSTEMS; SPACE WEATHER; FIELDS; SURFACE; NETWORK; EARTH AB [ 1] Pragmatic schemes for estimating geomagnetically induced current (GIC) values using different levels of knowledge about the physical quantities associated with the geomagnetic induction process are studied. The fundamental idea behind the proposed schemes is that as the knowledge about the detailed behavior of the relevant physical quantities decreases, the lack of knowledge is compensated by statistical characteristics of the geomagnetic induction process and GIC. It is shown that reasonable GIC estimates can be obtained if some information about the state of the geomagnetic environment is available. For example, single values of the time derivative of the magnetic field at the surface of the Earth or even a mere single value of the field deflection from the baseline level can sometimes be sufficient to give a reasonable statistical GIC estimate. It is also shown that the sampling rate of the magnetic field variations used to make the GIC estimates can be lowered down to about 60 s without crucially degrading the accuracy of the estimation. C1 NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Finnish Meteorol Inst, Space Res Unit, FIN-00101 Helsinki, Finland. Geol Survey Canada, Nat Resources Canada, Geomagnet Lab, Ottawa, ON K1A 0Y3, Canada. RP Pulkkinen, A (reprint author), NASA, Goddard Space Flight Ctr, Code 612-2, Greenbelt, MD 20771 USA. EM antti.pulkkinen@gsfc.nasa.gov; ari.viljanen@fmi.fi; rpirjola@NRCan.gc.ca NR 26 TC 26 Z9 26 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 AUG 29 PY 2006 VL 4 IS 8 AR S08005 DI 10.1029/2006SW000229 PG 15 WC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology & Atmospheric Sciences SC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology & Atmospheric Sciences GA 083FU UT WOS:000240442600001 ER PT J AU Webber, WR McDonald, FB Cummings, AC Stone, EC Heikkila, B Lal, N AF Webber, W. R. McDonald, F. B. Cummings, A. C. Stone, E. C. Heikkila, B. Lal, N. TI The disappearance of anomalous protons at Voyager 1 and Voyager 2 in the outer heliosphere between 1998 and 2002 SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article ID WIND TERMINATION SHOCK; COSMIC-RAY MODULATION; SOLAR-WIND; DISTANT HELIOSPHERE; ENHANCEMENTS; HELIOSHEATH; SPACECRAFT; HYDROGEN AB In 1998 and 1999 at V1 and V2 in the outer heliosphere between 55 and 75 AU, large intensities of anomalous H were observed with a peak in the differential energy spectrum at similar to 25 MeV. Subsequently, in 2000 and 2001 when these spacecraft were 5-10 AU further out, these intensities were greatly reduced by 11-year modulation effects, so that by the beginning of 2002 anomalous H had completely disappeared beneath the E-1.0 spectrum of galactic H at low energies. The modulation between 1998 and 2002 produced intensity changes of galactic H similar to those observed at the Earth in the same time period except that the changes at V1 and V2 were much smaller. The intensity change at V2 was also larger than that at V1. For anomalous H, however, the intensity changes at V1 and V2 were a factor of 10-20 times larger than those for galactic H, so that by the end of 2001 the anomalous H intensities were less than 1% of their 1998 values. Also, during one time period in late 2001 there was a large reduction of anomalous H at both V1 and V2 with no corresponding change in galactic H. These different intensity changes between galactic and anomalous H provide an insight into particle transport, drift, and acceleration processes in the region near the heliospheric termination shock, which is located just beyond V1. Radial gradient comparisons in 1998 and also at the times of reduced anomalous H intensities imply that most of the intensity reduction of anomalous H apparently occurred at similar to 90 AU or beyond. This could indicate source changes in the anomalous H spectra but most likely is a measure of changes in the "connection'' between V1 and V2 and the source region, such as might be caused by changing drift patterns and particle entry into the heliosphere. C1 New Mexico State Univ, Dept Astron, Las Cruces, NM 88003 USA. Univ Maryland, Inst Phys Sci & Technol, College Pk, MD 20742 USA. CALTECH, Downs Lab, Pasadena, CA 91125 USA. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Webber, WR (reprint author), New Mexico State Univ, Dept Astron, Las Cruces, NM 88003 USA. EM bwebber@nmsu.edu NR 24 TC 1 Z9 1 U1 0 U2 0 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0148-0227 J9 J GEOPHYS RES-SPACE JI J. Geophys. Res-Space Phys. PD AUG 26 PY 2006 VL 111 IS A8 AR A08107 DI 10.1029/2006JA011669 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 078KV UT WOS:000240102600001 ER PT J AU McCann, KM Yarrow, M DeVivo, A Mehrotra, P AF McCann, Karen M. Yarrow, Maurice DeVivo, Adrian Mehrotra, Piyush TI ScyFlow: an environment for the visual specification and execution of scientific workflows SO CONCURRENCY AND COMPUTATION-PRACTICE & EXPERIENCE LA English DT Article; Proceedings Paper CT GGF Workshop on Workflow in Grid Systems CY MAR 09, 2004 CL Berlin, GERMANY SP GGF DE grids; Grid computing; workflow; directed graph; distributed computing AB With the advent of Grid technologies, scientists and engineers are building more complex applications to utilize distributed Grid resources. Core Grid services provide a path for accessing and utilizing these resources in a secure and seamless fashion. However, what the scientists need is an environment that will allow them to specify their application runs at a high organizational level, and then will support efficient execution across any given set or sets of distributed resources. We have been designing and implementing ScyFlow, a dual-interface architecture, both Graphical User Interface (GUI) and Application Programming Interface (API), that addresses this problem. The scientist/user specifies the application tasks along with the necessary control and data flow, and then monitors and manages the execution of the resulting workflow across the distributed resources. In this paper, we utilize two scenarios to provide the details of the two modules of the project, the visual editor and the runtime workflow engine. Published in 2005 by John Wiley & Sons, Ltd. C1 NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. Comp Sci Corp, Lanham, MD 20706 USA. RP Mehrotra, P (reprint author), NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. EM piyush.mehrotra@nasa.gov NR 2 TC 3 Z9 3 U1 0 U2 0 PU JOHN WILEY & SONS LTD PI CHICHESTER PA THE ATRIUM, SOUTHERN GATE, CHICHESTER PO19 8SQ, W SUSSEX, ENGLAND SN 1532-0626 J9 CONCURR COMP-PRACT E JI Concurr. Comput.-Pract. Exp. PD AUG 25 PY 2006 VL 18 IS 10 BP 1155 EP 1167 DI 10.1002/cpe.990 PG 13 WC Computer Science, Software Engineering; Computer Science, Theory & Methods SC Computer Science GA 074IC UT WOS:000239804900008 ER PT J AU Wilmouth, DM Stimpfle, RM Anderson, JG Elkins, JW Hurst, DF Salawitch, RJ Lait, LR AF Wilmouth, D. M. Stimpfle, R. M. Anderson, J. G. Elkins, J. W. Hurst, D. F. Salawitch, R. J. Lait, L. R. TI Evolution of inorganic chlorine partitioning in the Arctic polar vortex SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID IN-SITU MEASUREMENTS; NASA ER-2 AIRCRAFT; PLUS CLO REACTION; LOWER STRATOSPHERE; OZONE LOSS; PRODUCT FORMATION; ANTARCTIC OZONE; 298 K; HO2; WINTER AB The first simultaneous, in situ atmospheric measurements of ClO, ClOOCl, ClONO2, and HCl, which together nearly compose total inorganic chlorine, Cl-y, were obtained using the NASA ER-2 aircraft, deployed from Kiruna, Sweden, during the SOLVE/THESEO mission. These chlorine measurements, along with Cly inferred from in situ measurements of organic chlorine source gases, offer an unprecedented opportunity to observe chlorine activation and recovery in the polar winter stratosphere and evaluate the inorganic chlorine budget, i.e., a test of the quantitative agreement between the sum of ClOx (ClO + 2 x ClOOCl), ClONO2, and HCl with Cl-y. Inside the Arctic vortex, inorganic chlorine is rarely fully activated with ClOx/Cl-y ranging from approximately 0.25 to 0.90. An apparent discrepancy in the inorganic chlorine budget for much of the midwinter correlates well with back trajectory solar zenith angle minimum and is consistent with the presence of Cl-2, which was not observable. Evaluation of the midwinter inorganic chlorine budget, excluding data where Cl-2 is present, yields (ClOx + ClONO2 + HCl)/Cl-y = 0.94 +/- 0.07. In contrast, a shortfall in the late winter inorganic chlorine budget is the result of an apparent low bias in the HCl measurements. A diurnal box model constructed to analyze chlorine recovery rates highlights the importance of not only the Cl + CH4 reaction in HCl formation, but also OH + ClO and potentially HO2 + ClO. We find that significant HCl production accompanied net ClONO2 production in the inorganic chlorine recovery phase of this Arctic winter. C1 Harvard Univ, Dept Chem & Biol Chem, Cambridge, MA 02138 USA. NOAA, Global Monitoring Div, Earth Syst Res Lab, Boulder, CO 80305 USA. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Wilmouth, DM (reprint author), Harvard Univ, Dept Chem & Biol Chem, Cambridge, MA 02138 USA. EM wilmouth@huarp.harvard.edu RI Salawitch, Ross/B-4605-2009; Hurst, Dale/D-1554-2016 OI Salawitch, Ross/0000-0001-8597-5832; Hurst, Dale/0000-0002-6315-2322 NR 46 TC 9 Z9 9 U1 2 U2 6 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD AUG 25 PY 2006 VL 111 IS D16 AR D16308 DI 10.1029/2005JD006951 PG 16 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 078KA UT WOS:000240100400007 ER PT J AU Worden, J Bowman, K Noone, D Beer, R Clough, S Eldering, A Fisher, B Goldman, A Gunson, M Herman, R Kulawik, SS Lampel, M Luo, M Osterman, G Rinsland, C Rodgers, C Sander, S Shephard, M Worden, H AF Worden, John Bowman, Kevin Noone, David Beer, Reinhard Clough, Shepard Eldering, Annmarie Fisher, Brendan Goldman, Aaron Gunson, Michael Herman, Robert Kulawik, Susan S. Lampel, Michael Luo, Ming Osterman, Gregory Rinsland, Curtis Rodgers, Clive Sander, Stanley Shephard, Mark Worden, Helen TI Tropospheric emission spectrometer observations of the tropospheric HDO/H2O ratio: Estimation approach and characterization SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID INFRARED SOLAR SPECTRA; WATER-VAPOR; ISOTOPE RATIOS; ART.; RETRIEVALS; SIMULATION; TRANSPORT; DEUTERIUM; TRACERS; MOZART AB [ 1] We present global, vertical profile estimates of the HDO/H2O ratio from the Tropospheric Emission Spectrometer ( TES) on the Earth Observing System ( EOS) Aura satellite. We emphasize in this paper the estimation approach and error characterization, which are critical to determining the very small absolute concentration of HDO relative to H2O and its uncertainty. These estimates were made from TES nadir-viewing ( downlooking) thermal infrared spectral radiances observed on 20 September 2004. Profiles of HDO and H2O are simultaneously estimated from the observed radiances and a profile of the ratio is then calculated. This simultaneous, or "joint,'' estimate is regularized with an a priori covariance matrix that includes expected correlations between HDO and H2O. This approach minimizes errors in the profile of the HDO/H2O ratio that are due to overlapping HDO and H2O spectroscopic lines. Under clear-sky conditions in the tropics, TES estimates of the HDO/H2O ratio are sensitive to the distribution of the actual ratio between the surface and about 300 hPa with peak sensitivity at 700 hPa. The sensitivity decreases with latitude through its dependence on temperature and water amount. We estimate a precision of approximately 1% to 2% for the ratio of the HDO/H2O tropospheric densities; however, there is possibly a bias of approximately 5% in the ratio due to the HDO spectroscopic line strengths. These global observations clearly show increased isotopic depletion of water vapor at higher latitudes as well as increased depletion in the upper troposphere versus the lower troposphere. C1 CALTECH, Jet Prop Lab, Div Earth & Space Sci, Pasadena, CA 91109 USA. Univ Colorado, PAOS, Boulder, CO 80309 USA. Univ Colorado, CIRES, Boulder, CO 80309 USA. Atmospher & Environm Res Inc, Lexington, MA 02421 USA. Univ Denver, Dept Phys, Denver, CO 80208 USA. Raytheon Informat Solut, Pasadena, CA 91101 USA. NASA, Langley Res Ctr, Hampton, VA 23681 USA. Univ Oxford, Clarendon Lab, Oxford OX1 3PU, England. RP Worden, J (reprint author), CALTECH, Jet Prop Lab, Div Earth & Space Sci, 4800 Oak Grove Dr,MS 183-301, Pasadena, CA 91109 USA. EM john.worden@jpl.nasa.gov NR 24 TC 84 Z9 88 U1 1 U2 15 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 AUG 25 PY 2006 VL 111 IS D16 AR D16309 DI 10.1029/2005JD006606 PG 10 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 078KA UT WOS:000240100400002 ER PT J AU Lissauer, JJ AF Lissauer, Jack J. TI Growing apart in lock step SO SCIENCE LA English DT Editorial Material ID PLUTO; ORIGIN C1 NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Lissauer, JJ (reprint author), NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. EM jlissauer@mail.arc.nasa.gov NR 9 TC 1 Z9 1 U1 0 U2 0 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 AUG 25 PY 2006 VL 313 IS 5790 BP 1054 EP 1055 DI 10.1126/science.1128447 PG 2 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 076ZT UT WOS:000239998200025 PM 16931743 ER PT J AU Nakagawa, YE Yoshida, A Sugita, S Tanaka, K Ishikawa, N Tamagawa, T Suzuki, M Shirasaki, Y Kawai, N Matsuoka, M Atteia, JL Pelangeon, A Vanderspek, R Crew, GB Villasenor, JS Butler, N Doty, JP Ricker, GR Pizzichini, G Donaghy, TQ Lamb, DQ Graziani, C Sato, R Maetou, M Arimoto, M Kotoku, J Jernigan, JG Sakamoto, T Olive, JF Boer, M Fenimore, EE Galassi, M Woosley, SE Yamauchi, M Takagishi, K Hatsukade, I AF Nakagawa, Yujin E. Yoshida, Atsumasa Sugita, Satoshi Tanaka, Kaoru Ishikawa, Nobuyuki Tamagawa, Toru Suzuki, Motoko Shirasaki, Yuji Kawai, Nobuyuki Matsuoka, Masaru Atteia, Jean-Luc Pelangeon, Alexandre Vanderspek, Roland Crew, Geoffrey B. Villasenor, Joel S. Butler, Nat Doty, John P. Ricker, George R. Pizzichini, Graziella Donaghy, Timothy Q. Lamb, Donald Q. Graziani, Carlo Sato, Rie Maetou, Miki Arimoto, Makoto Kotoku, Jun'ichi Jernigan, J. Garrett Sakamoto, Takanori Olive, Jean-Francois Boer, Michel Fenimore, Edward E. Galassi, Mark Woosley, Stanford E. Yamauchi, Makoto Takagishi, Kunio Hatsukade, Isamu TI An optically dark GRB observed by HETE-2: GRB 051022 SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN LA English DT Letter DE gamma rays : observations; star : individual (GRB 051022); X-rays : ISM ID GAMMA-RAY BURSTS; ABSORPTION; BEPPOSAX; ENERGY; AFTERGLOWS; ENERGETICS; SPECTRUM; UNIVERSE; PROMPT; GALAXY AB GRB 051022 was detected at 13:07:58 on 2005 October 22 UT by HETE-2. The location of GRB 051022 was determined immediately by the fight localization system. This burst contained multiple pulses, and had a rather long duration of about 190 s. The detections of candidate X-ray and radio afterglows were reported, whereas no optical afterglow was found. Optical spectroscopic observations of the host galaxy revealed a redshift of z = 0.8. Using data derived by a HETE-2 observation of the prompt emission, we found absorption of N-H = (8.8(-2.9)(+3.1)) x 10(22) cm(-2) and visual extinction of A(V) = 49(-16)(+17) mag in the host galaxy. If this is the case, no detection of any optical transient would be quite reasonable. The absorption derived by Swift XRT observations of the afterglow is fully consistent with those obtained from an early HETE-2 observation of the prompt emission. Our analysis implies an interpretation that the absorbing medium may be outside the external shock at R similar to 10(16) cm, which could be a dusty molecular cloud. C1 Aoyama Gakuin Univ, Dept Math & Phys, Sagamihara, Kanagawa 2298558, Japan. RIKEN, Inst Phys & Chem Res, Wako, Saitama 3510198, Japan. Tokyo Inst Technol, Dept Phys, Meguro Ku, Tokyo 1528551, Japan. Natl Astron Observ Japan, Mitaka, Tokyo 1818588, Japan. JAXA, Tsukuba Space Ctr, Tsukuba, Ibaraki 3058505, Japan. Observ Midi Pyrenees, LAT, F-31400 Toulouse, France. MIT, Ctr Space Res, Cambridge, MA 02139 USA. Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. Noqsi Aerosp Ltd, Pine, CO 80470 USA. IASF Bologna, INAF, I-40129 Bologna, Italy. Univ Chicago, Ctr Astron & Astrophys, Chicago, IL 60637 USA. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Observ Midi Pyrenees, Ctr Etud Spatiale Rayonnements, F-31028 Toulouse 4, France. Los Alamos Natl Lab, Los Alamos, NM 87545 USA. Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA. Miyazaki Univ, Fac Engn, Miyazaki 8892192, Japan. RP Nakagawa, YE (reprint author), Aoyama Gakuin Univ, Dept Math & Phys, 5-10-1 Fuchinobe, Sagamihara, Kanagawa 2298558, Japan. EM yujin@phys.aoyama.ac.jp NR 50 TC 9 Z9 9 U1 1 U2 1 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0004-6264 EI 2053-051X J9 PUBL ASTRON SOC JPN JI Publ. Astron. Soc. Jpn. PD AUG 25 PY 2006 VL 58 IS 4 BP L35 EP L39 DI 10.1093/pasj/58.4.L35 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 082GZ UT WOS:000240376000003 ER PT J AU Huang, FT Mayr, HG Reber, CA Russell, J Mlynczak, M Mengel, J AF Huang, Frank T. Mayr, Hans G. Reber, Carl A. Russell, James Mlynczak, Marty Mengel, John TI Zonal-mean temperature variations inferred from SABER measurements on TIMED compared with UARS observations SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article ID ATMOSPHERE RESEARCH SATELLITE; DOPPLER-SPREAD PARAMETERIZATION; WAVE MOMENTUM DEPOSITION; MIDDLE ATMOSPHERE; GRAVITY-WAVES; LOWER THERMOSPHERE; EQUATORIAL MESOSPHERE; TIDES; OSCILLATIONS; SIMULATION AB In the zonal mean meridional winds of the upper mesosphere, oscillations with periods between 1 and 4 months have been inferred from UARS measurements and independently predicted with the Numerical Spectral Model (NSM). The wind oscillations tend to be confined to low latitudes and appear to be driven, at least in part, by wave-mean-flow interactions. Winds across the equator should generate, due to dynamical heating and cooling, temperature oscillations with opposite phase in the two hemispheres. Investigating this phenomenon, we have analyzed SABER temperatures from TIMED in the altitude range between 55 and 95 km to delineate with an empirical model, the yearlong variability of the migrating tides and zonal mean components. The inferred seasonal variations of the diurnal tide, characterized by amplitude maxima near equinox, are in substantial agreement with UARS observations and results from the NSM. For the zonal mean, the dominant seasonal variations in the SABER temperatures, with annual (12 months) and semiannual (6 months) periodicities, agree well with those derived from UARS measurements. The intraseasonal variations with periods between 2 and 4 months have amplitudes close to 2 K, almost half as large as those for the dominant seasonal variations. Their amplitudes are in qualitative agreement with the corresponding values inferred from UARS during different years. The SABER and UARS temperature variations reveal pronounced hemispherical asymmetries, consistent with meridional wind oscillations across the equator. The phase of the semiannual temperature oscillations from the NSM agrees with the observations from UARS and SABER. However, the amplitudes are systematically smaller, which may indicate that planetary waves are more important than is allowed for in the model. For the shorter-period intraseasonal variations, which can be generated by gravity wave drag, the model results are generally in better agreement with the observations. C1 Creat Comp Solut Inc, Rockville, MD 20850 USA. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. NASA, Langley Res Ctr, Hampton, VA 23681 USA. Hampton Univ, Ctr Atmospher Sci, Hampton, VA 23668 USA. Sci Syst & Applicat, Lanham, MD 20706 USA. RP Huang, FT (reprint author), Creat Comp Solut Inc, Rockville, MD 20850 USA. EM fthuang@comcast.net RI Mlynczak, Martin/K-3396-2012 NR 33 TC 17 Z9 17 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 AUG 24 PY 2006 VL 111 IS A10 AR A10S07 DI 10.1029/2005JA011427 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 078KX UT WOS:000240102800001 ER PT J AU Tsurutani, BT McPherron, RL Gonzalez, WD Lu, G Sobral, JHA Gopalswamy, N AF Tsurutani, B. T. McPherron, R. L. Gonzalez, W. D. Lu, G. Sobral, J. H. A. Gopalswamy, N. TI Introduction to special section on corotating solar wind streams and recurrent geomagnetic activity (vol 111, art no A08S90, 2006) SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Correction C1 CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. Univ Calif Los Angeles, Inst Geophys & Planetary Phys, Los Angeles, CA 90024 USA. Natl Inst Space Res, Sao Paulo, Brazil. Natl Ctr Atmospher Res, High Altitude Observ, Boulder, CO 80307 USA. NASA, Goddard Space Flight Ctr, Extraterr Phys Lab, Greenbelt, MD 20771 USA. RP Tsurutani, BT (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91125 USA. RI Gopalswamy, Nat/D-3659-2012 NR 1 TC 1 Z9 1 U1 0 U2 0 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0148-0227 J9 J GEOPHYS RES-SPACE JI J. Geophys. Res-Space Phys. PD AUG 24 PY 2006 VL 111 IS A8 AR A08S90 DI 10.1029/2006JA011980 PG 1 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 078KS UT WOS:000240102300004 ER PT J AU Schawinski, K Khochfar, S Kaviraj, S Yi, SK Boselli, A Barlow, T Conrow, T Forster, K Friedman, PG Martin, DC Morrissey, P Neff, S Schiminovich, D Seibert, M Small, T Wyder, TK Bianchi, L Donas, J Heckman, T Lee, YW Madore, B Milliard, B Rich, RM Szalay, A AF Schawinski, Kevin Khochfar, Sadegh Kaviraj, Sugata Yi, Sukyoung K. Boselli, Alessandro Barlow, Tom Conrow, Tim Forster, Karl Friedman, Peter G. Martin, D. Chris Morrissey, Patrick Neff, Susan Schiminovich, David Seibert, Mark Small, Todd Wyder, Ted K. Bianchi, Luciana Donas, Jose Heckman, Tim Lee, Young-Wook Madore, Barry Milliard, Bruno Rich, R. Michael Szalay, Alex TI Suppression of star formation in early-type galaxies by feedback from supermassive black holes SO NATURE LA English DT Article ID DIGITAL SKY SURVEY; EVOLUTION-EXPLORER; GALACTIC NUCLEI; MERGERS; QUASARS; COLORS; ORIGIN AB Detailed high-resolution observations of the innermost regions of nearby galaxies have revealed the presence of supermassive black holes(1-4). These black holes may interact with their host galaxies by means of 'feedback' in the form of energy and material jets; this feedback affects the evolution of the host and gives rise to observed relations between the black hole and the host(5). Here we report observations of the ultraviolet emissions of massive early-type galaxies. We derive an empirical relation for a critical black-hole mass ( as a function of velocity dispersion) above which the outflows from these black holes suppress star formation in their hosts by heating and expelling all available cold gas. Supermassive black holes are negligible in mass compared to their hosts but nevertheless seem to play a critical role in the star formation history of galaxies. C1 Yonsei Univ, Ctr Space Astrophys, Seoul 120749, South Korea. Univ Oxford, Dept Phys, Oxford OX1 3RH, England. Lab Astrophys Marseille, F-13376 Marseille, France. CALTECH, Pasadena, CA 91125 USA. NASA, Goddard Space Flight Ctr, Astron & Solar Phys Lab, Greenbelt, MD 20771 USA. Columbia Univ, Dept Astron, New York, NY 10027 USA. Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. Carnegie Inst Washington Observ, Pasadena, CA 91101 USA. Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA. RP Yi, SK (reprint author), Yonsei Univ, Ctr Space Astrophys, Seoul 120749, South Korea. EM yi@yonsei.ac.kr OI Schawinski, Kevin/0000-0001-5464-0888 NR 25 TC 85 Z9 85 U1 0 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 AUG 24 PY 2006 VL 442 IS 7105 BP 888 EP 891 DI 10.1038/nature04934 PG 4 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 076LT UT WOS:000239960500030 PM 16929291 ER PT J AU Jimenez, C Pumphrey, HC MacKenzie, IA Manney, GL Santee, ML Schwartz, MJ Harwood, RS Waters, JW AF Jimenez, C. Pumphrey, H. C. MacKenzie, I. A. Manney, G. L. Santee, M. L. Schwartz, M. J. Harwood, R. S. Waters, J. W. TI EOS MLS observations of dehydration in the 2004-2005 polar winters SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID AURA SATELLITE; STRATOSPHERE; VORTEX AB Observations of water vapour and temperature from the Earth Observing System Microwave Limb Sounder are used to study dehydration in the 2004 and 2005 polar vortices. Significant differences were found for the Antarctic winters, with the 2005 vortex colder and more extensively dehydrated. For the 2005 winter water vapour reductions were observed from mid-June, coincident with a decrease in temperatures, extending vertically between similar to 12-21 km. Reductions of up to similar to 3 ppmv in water vapour were recorded a month later. Permanent dehydration was apparent between similar to 15-20 km, where 3 months later the temperature recovery was not followed by a recovery in water vapour. The 2004-2005 Arctic winter was unusually cold, but only one single event of depleted water vapour at the end of January was linked to ice formation. For this event, a reduction of up to similar to 0.5 ppmv was observed over Spitsbergen between similar to 12-20 km. C1 Univ Edinburgh, Sch Geosci, Edinburgh EH9 3JN, Midlothian, Scotland. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. New Mexico Inst Min & Technol, Dept Phys, Socorro, NM 87801 USA. RP Jimenez, C (reprint author), Univ Edinburgh, Sch Geosci, Crew Bldg,Mayfield Rd, Edinburgh EH9 3JN, Midlothian, Scotland. EM carlos.jimenez@ed.ac.uk RI mackenzie, ian/E-9320-2013; Schwartz, Michael/F-5172-2016 OI Schwartz, Michael/0000-0001-6169-5094 NR 15 TC 17 Z9 17 U1 0 U2 6 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 AUG 23 PY 2006 VL 33 IS 16 AR L16806 DI 10.1029/2006GL025926 PG 4 WC Geosciences, Multidisciplinary SC Geology GA 078JP UT WOS:000240099300001 ER PT J AU Signorini, SR Garcia, VMT Piola, AR Garcia, CAE Mata, MM McClain, CR AF Signorini, Sergio R. Garcia, Virginia M. T. Piola, Alberto R. Garcia, Carlos A. E. Mata, Mauricio M. McClain, Charles R. TI Seasonal and interannual variability of calcite in the vicinity of the Patagonian shelf break (38 degrees S-52 degrees S) SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID WESTERN SOUTH-ATLANTIC; EMILIANIA-HUXLEYI; CHLOROPHYLL-A; COCCOLITHOPHORE; OCEAN; PHYTOPLANKTON; SURFACE; HYDROGRAPHY; BLOOMS AB The timing and duration of coccolithophore blooms along the Patagonian shelf break, as well as insights on the mechanisms that drive and maintain these blooms, were analyzed using time series of chlorophyll chl alpha, calcite, and sea-surface temperature (SST) derived from remote sensing data (SeaWiFS and AVHRR) and historic hydrographic data. The seasonal variability and succession of phytoplankton groups respond to light intensity and nutrient supply within the mixed layer due to seasonal changes in stratification. The early spring bloom is diatom-dominated and starts in September under nutrient-rich Malvinas waters when the mixed layer begins to shallow (< 80 m), and peaks around November with mixed layer depths (MLD) less than 40 m. After nutrient depletion from the spring bloom, a coccolithophore bloom begins in November when the MLD is less than 40 m, and peaks in January when the MLD reaches its minimum (18 m) and PAR reaches its maximum intensity. C1 NASA, Sci Applicat Int Corp, NASA Earth Sci Support, Goddard Space Flight Ctr, Beltsville, MD 20705 USA. Fed Univ Rio Grande, Dept Oceanog, BR-96201900 Rio Grande, RS, Brazil. Serv Hidrog Naval, Buenos Aires, DF, Argentina. Univ Buenos Aires, Buenos Aires, DF, Argentina. Fed Univ Rio Grande, Dept Phys, BR-96201900 Rio Grande, RS, Brazil. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Signorini, SR (reprint author), NASA, Sci Applicat Int Corp, NASA Earth Sci Support, Goddard Space Flight Ctr, 4600 Powder Mill Rd, Beltsville, MD 20705 USA. EM sergio@simbios.gsfc.nasa.gov RI Tavano, Virginia/C-5241-2013; Piola, Alberto/O-2280-2013; Garcia, Carlos/K-7382-2012; Mata, Mauricio/H-4605-2011 OI Tavano, Virginia/0000-0003-0039-8111; Piola, Alberto/0000-0002-5003-8926; Mata, Mauricio/0000-0002-9028-8284 NR 26 TC 26 Z9 26 U1 0 U2 1 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD AUG 23 PY 2006 VL 33 IS 16 AR L16610 DI 10.1029/2006GL026592 PG 5 WC Geosciences, Multidisciplinary SC Geology GA 078JP UT WOS:000240099300004 ER PT J AU Aumann, HH Broberg, S Elliott, D Gaiser, S Gregorich, D AF Aumann, H. H. Broberg, Steve Elliott, Denis Gaiser, Steve Gregorich, Dave TI Three years of Atmospheric Infrared Sounder radiometric calibration validation using sea surface temperatures SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID AIRS; CLIMATE; OCEAN; MODEL AB This paper evaluates the absolute accuracy and stability of the radiometric calibration of the Atmospheric Infrared Sounder (AIRS) by analyzing the difference between the brightness temperatures measured at 2616 cm(-1) and those calculated at the top of the atmosphere (TOA), using the Real-Time Global Sea Surface Temperature (RTGSST) for cloud-free night tropical oceans between +/-30 degrees latitude. The TOA correction is based on radiative transfer. The analysis of the first 3 years of AIRS radiances verifies the absolute calibration at 2616 cm(-1) to better than 200 mK, with better than 16 mK/yr stability. The AIRS radiometric calibration uses an internal full aperture wedge blackbody with the National Institute of Standards and Technology (NIST) traceable prelaunch calibration coefficients. The calibration coefficients have been unchanged since launch. The analysis uses very tight cloud filtering, which selects about 7000 cloud-free tropical ocean spectra per day, about 0.5% of the data. The absolute accuracy and stability of the radiometry demonstrated at 2616 cm(-1) are direct consequences of the implementation of AIRS as a thermally controlled, cooled grating-array spectrometer and meticulous attention to details. Comparable radiometric performance is inferred from the AIRS design for all 2378 channels. AIRS performance sets the benchmark for what can be achieved with a state-of-the-art hyperspectral radiometer from polar orbit and what is expected from future hyperspectral sounders. AIRS was launched into a 705 km altitude polar orbit on NASA's Earth Observation System (EOS) Aqua spacecraft on 4 May 2002. AIRS covers the 3.7-15.4 micron region of the thermal infrared spectrum with a spectral resolution of nu/Delta nu = 1200 and has returned 3.7 million spectra of the upwelling radiance each day since the start of routine data gathering in September 2002. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Aumann, HH (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM aumann@jpl.nasa.gov NR 19 TC 53 Z9 54 U1 0 U2 2 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X EI 2169-8996 J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD AUG 23 PY 2006 VL 111 IS D16 AR D16S90 DI 10.1029/2005JD006822 PG 8 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 078JZ UT WOS:000240100300004 ER PT J AU Feely, RA Takahashi, T Wanninkhof, R McPhaden, MJ Cosca, CE Sutherland, SC Carr, ME AF Feely, R. A. Takahashi, T. Wanninkhof, R. McPhaden, M. J. Cosca, C. E. Sutherland, S. C. Carr, Mary-Elena TI Decadal variability of the air-sea CO2 fluxes in the equatorial Pacific Ocean SO JOURNAL OF GEOPHYSICAL RESEARCH-OCEANS LA English DT Article ID 1997-98 EL-NINO; INTERANNUAL VARIABILITY; NORTH PACIFIC; WATER; TEMPERATURE; CIRCULATION; PCO(2); ENSO; DISTRIBUTIONS; OSCILLATION AB In order to determine the interannual and decadal changes in the air-sea carbon fluxes of the equatorial Pacific, we developed seasonal and interannual relationships between the fugacity of CO2 (fCO(2)) and sea surface temperature (SST) from shipboard data that were applied to high-resolution temperature fields deduced from satellite data to obtain high-resolution large-scale estimates of the regional fluxes. The data were gathered on board research ships from November 1981 through June 2004 between 95 degrees W and 165 degrees E. The distribution of fCO(2sw) during five El Nino periods and four La Nina periods were documented. Observations made during the warm boreal winter-spring season and during the cooler boreal summer-fall season of each year enabled us to examine the interannual and seasonal variability of the fCO(2sw)-SST relationships. A linear fit through all of the data sets yields an inverse correlation between SST and fCO(2sw), with both interannual and seasonal differences in slope. On average, the surface water fCO(2) in the equatorial region has been increasing at a rate similar to the atmospheric CO2 increase. In addition, there appears to be a slight increase (similar to 27%) in the outgassing flux of CO2 after the 1997-1998 Pacific Decadal Oscillation (PDO) regime shift. Most of this flux increase is due to increase in wind speeds after the spring of 1998, although increases in fCO(2sw) after 1998 are also important. These increases are coincident with the recent rebound of the shallow water meridional overturning circulation in the tropical and subtropical Pacific after the regime shift. C1 NOAA, Pacific Marine Environm Lab, Seattle, WA 98115 USA. Columbia Univ, Lamont Doherty Earth Observ, Palisades, NY 10964 USA. NOAA, Atlantic Oceanog & Meteorol Lab, Miami, FL 33149 USA. CALTECH, Jet Prop Lab, Pasadena, CA 91101 USA. RP Feely, RA (reprint author), NOAA, Pacific Marine Environm Lab, Bin C15700,7600 Sand Point Way NE, Seattle, WA 98115 USA. EM richard.a.feely@noaa.gov RI McPhaden, Michael/D-9799-2016 NR 47 TC 79 Z9 81 U1 5 U2 24 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0148-0227 J9 J GEOPHYS RES-OCEANS JI J. Geophys. Res.-Oceans PD AUG 23 PY 2006 VL 111 IS C8 AR C08S90 DI 10.1029/2005JC003129 PG 16 WC Oceanography SC Oceanography GA 078KI UT WOS:000240101300001 ER PT J AU Frey, HV AF Frey, H. V. TI Impact constraints on, and a chronology for, major events in early Mars history SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Article ID CRUSTAL MAGNETIC-FIELD; DICHOTOMY BOUNDARY; HEMISPHERIC DICHOTOMY; GLOBAL SURVEYOR; PLATE-TECTONICS; GIANT IMPACT; EVOLUTION; BASIN; ORIGIN; TOPOGRAPHY AB Large-diameter visible and buried impact basins, seen as "quasi-circular depressions'' (QCDs) in MOLA gridded data, provide a self-consistent chronology for major events on early Mars in terms of N(200) crater retention ages. On the basis of a conversion to model absolute ages, this chronology extends back hundreds of millions of years into a previously unknown "pre-Noachian'' epoch during which a now buried highlands surface was established, in which several very large impact basins formed while the global magnetic field was still present. A cluster of very large "lowland-making'' basins occurred at a model age of about 4.13 GY (or earlier), forming the fundamental topography of the Mars crustal dichotomy at a time prior to the age of the oldest visible highland crust. This early event in Martian history marks the transition from the "pre-Noachian'' to the Early Noachian when the well-preserved Hellas, Argyre, and Isidis basins formed, all after the global magnetic field died. C1 NASA, Goddard Space Flight Ctr, Planetary Geodynam Lab, Greenbelt, MD 20771 USA. RP Frey, HV (reprint author), NASA, Goddard Space Flight Ctr, Planetary Geodynam Lab, Mail Code 921, Greenbelt, MD 20771 USA. EM herbert.v.frey@nasa.gov NR 59 TC 55 Z9 55 U1 0 U2 7 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9097 EI 2169-9100 J9 J GEOPHYS RES-PLANET JI J. Geophys. Res.-Planets PD AUG 23 PY 2006 VL 111 IS E8 AR E08ZS91 DI 10.1029/2005JE002449 PG 11 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 078KK UT WOS:000240101500001 ER PT J AU Luz, D Civeit, T Courtin, R Lebreton, JP Gautier, D Witasse, O Kaufer, A Ferri, F Lara, L Livengood, T Kostiuk, T AF Luz, D. Civeit, T. Courtin, R. Lebreton, J. -P. Gautier, D. Witasse, O. Kaufer, A. Ferri, F. Lara, L. Livengood, T. Kostiuk, T. TI Characterization of zonal winds in the stratosphere of Titan with UVES: 2. Observations coordinated with the Huygens Probe entry SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Article ID TROPOSPHERIC CLOUDS; ATMOSPHERE; TEMPERATURES; OCCULTATION; DYNAMICS AB The Huygens Probe has successfully entered Titan's atmosphere and landed on its surface on 14 January 2005. With the aim of characterizing the zonal wind flow in Titan's stratosphere close to the time of entry, coordinated observations were carried out at the Very Large Telescope on the nights of 7, 12, 14, and 15 January. As in our previous investigation (Luz et al., 2005), we used the UVES instrument, mounted on the Kueyen-UT2 telescope, simultaneously achieving high spectral resolving power and high spatial resolution. The field has been derotated in order to align the 0.3-arcsec aperture perpendicularly to Titan's rotation axis. In this configuration, spatial information in the east-west direction is preserved in a set of spectra in the direction perpendicular to dispersion. We present measurements of zonal winds obtained with the technique of absolute accelerometry. The observations were made in the wavelength range 4200-6200 angstrom, probing between 115 and 280 km, with peak contributions at 200 and 170 km for the lower and upper parts of the domain. We detect prograde zonal winds with lower limits 46 and 53 ms(-1) at these altitudes. These values are close to our previous measurements. C1 Univ Lisbon, Ctr Astron & Astrofis, Observ Astron Lisboa, P-1349018 Lisbon, Portugal. Observ Paris, Sect Meudon, Lab Etud Spatiales & Instrumentat Astrophys, F-92195 Meudon, France. European Space Agcy, Estec, Res & Sci Support Dept, NL-2200 AG Noordwijk, Netherlands. European So Observ, Santiago 19, Chile. Univ Padua, CISAS, I-35131 Padua, Italy. CSIC, Inst Astrofis Andalucia, E-18008 Granada, Spain. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Luz, D (reprint author), Univ Lisbon, Ctr Astron & Astrofis, Observ Astron Lisboa, P-1349018 Lisbon, Portugal. EM dluz@oal.ul.pt RI Livengood, Timothy/C-8512-2012; Luz, David/J-4588-2013; Kostiuk, Theodor/A-3077-2014 OI Luz, David/0000-0002-9473-8035; NR 30 TC 8 Z9 8 U1 1 U2 2 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9097 EI 2169-9100 J9 J GEOPHYS RES-PLANET JI J. Geophys. Res.-Planets PD AUG 23 PY 2006 VL 111 IS E8 AR E08S90 DI 10.1029/2005JE002617 PG 8 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 078KK UT WOS:000240101500002 ER PT J AU Kunhikrishnan, T Lawrence, MG von Kuhlmann, R Wenig, MO Asman, WAH Richter, A Burrows, JP AF Kunhikrishnan, T. Lawrence, Mark G. von Kuhlmann, Rolf Wenig, Mark O. Asman, Willem A. H. Richter, Andreas Burrows, John P. TI Regional NOx emission strength for the Indian subcontinent and the impact of emissions from India and neighboring countries on regional O-3 chemistry SO NEW JOURNAL OF PHYSICS LA English DT Article ID MOZAIC AIRBORNE PROGRAM; IN-SERVICE AIRCRAFT; TROPOSPHERIC OZONE; AIR-POLLUTION; NONMETHANE HYDROCARBONS; SATELLITE-OBSERVATIONS; GLOBAL DISTRIBUTIONS; URBAN ATMOSPHERE; NORTH-AMERICA; ASIA AB This study examines the regional NOx emission strength and influence of external emissions on O-3-related chemistry over the Indian subcontinent based on a three-dimensional chemistry transport model and space-based observations, following up on our earlier work on NOx chemistry over southern Asia. NOx mass and emissions from Global Ozone Monitoring Experiment (GOME) and Model of Atmospheric Transport and Chemistry-Max Planck Institute for Chemistry Version (MATCH-MPIC) over India are compared, and the uncertainties in the estimates are briefly discussed. This study also employs the concept of small-perturbation tendencies to compute the scaled sensitivities with modified NOx emissions for India and the neighboring continents. The sensitivities of NOx, O-3, OH, and reservoir species of NOx over India to NOx emission from India, Southeast Asia, Africa, China, and the Middle East are discussed with respect to the photochemistry and the regional meteorology. Our study suggests that the mean regional NOx emission strength for India is close to 2.5 Tg(N)/yr with a seasonal maximum (similar to 3 Tg(N)/yr) during April and minimum (similar to 1.6 Tg(N)/yr) during winter. The changes in the O-3 concentrations with respect to NOx and nonmethane hydrocarbon emissions from India show that southern India is relatively more sensitive to local emission. C1 Max Planck Inst Chem, Dept Atmospher Chem, D-55020 Mainz, Germany. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Univ Bremen, Dept Environm Phys & Remote Sensing, D-28359 Bremen, Germany. RP Kunhikrishnan, T (reprint author), NASA, Langley Res Ctr, Atmospher Sci Directorate, 100 NASA Rd, Hampton, VA 23681 USA. EM kunhi@larc.nasa.gov RI Richter, Andreas/C-4971-2008; Wenig, Mark/K-7279-2012 OI Richter, Andreas/0000-0003-3339-212X; NR 52 TC 0 Z9 0 U1 1 U2 8 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 AUG 23 PY 2006 VL 8 AR D15301 DI 10.1029/2005JD006036 PG 16 WC Physics, Multidisciplinary SC Physics GA 077JJ UT WOS:000240024800001 ER PT J AU Weber, AL Pizzarello, S AF Weber, Arthur L. Pizzarello, Sandra TI The peptide-catalyzed stereospecific synthesis of tetroses: A possible model for prebiotic molecular evolution SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF AMERICA LA English DT Article DE prebiotic chemistry; chirality; catalysis ID ASYMMETRIC ALDOL REACTIONS; AMINO-ACIDS; PROLINE; ENZYME; METEORITES; ALDEHYDES AB Using a water-based prebiotic model of sugar synthesis involving glycolaidehyde self-condensation, we demonstrate that homochiral L-clipepticle catalysts lead to the stereospecific syntheses of tetroses. The asymmetric effect is largest for erythrose, which may reach a D-enantiomeric excess of > 80% with L-Val-L-Val catalyst. Based on results obtained with various peptides, we propose a possible catalytic-reaction intermediate, consisting of an imidazolidinone ring formed between the two nitrogen atoms of the peptide catalyst and the C1 of one glycolalclehyde molecule. The study was motivated by the premise that exogenous material, such as the nonracemic amino acids found in meteorites, could have participated in the terrestrial evolution of molecular asymmetry by stereospecific catalysis. Because peptides might have formed readily on the early Earth, it is possible that their catalytic contribution was relevant in the prebiotic processes that preceded the onset of life. C1 Arizona State Univ, Dept Chem & Biochem, Tempe, AZ 85018 USA. NASA, Ames Res Ctr, SETI Inst, Moffett Field, CA 94035 USA. RP Pizzarello, S (reprint author), Arizona State Univ, Dept Chem & Biochem, Tempe, AZ 85018 USA. EM pizzar@asu.edu NR 27 TC 58 Z9 60 U1 1 U2 19 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 AUG 22 PY 2006 VL 103 IS 34 BP 12713 EP 12717 DI 10.1073/pnas.0602320103 PG 5 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 077NI UT WOS:000240035900014 PM 16905650 ER PT J AU van der Werf, GR Randerson, JT Giglio, L Collatz, GJ Kasibhatla, PS Arellano, AF AF van der Werf, G. R. Randerson, J. T. Giglio, L. Collatz, G. J. Kasibhatla, P. S. Arellano, A. F., Jr. TI Interannual variability in global biomass burning emissions from 1997 to 2004 SO ATMOSPHERIC CHEMISTRY AND PHYSICS LA English DT Article ID ATMOSPHERIC CARBON-DIOXIDE; NET PRIMARY PRODUCTION; FIRE RADIATIVE ENERGY; SOUTHERN AFRICA; SPOT-VEGETATION; FOREST-FIRES; MODIS; ECOSYSTEMS; SAVANNA; DATASET AB Biomass burning represents an important source of atmospheric aerosols and greenhouse gases, yet little is known about its interannual variability or the underlying mechanisms regulating this variability at continental to global scales. Here we investigated fire emissions during the 8 year period from 1997 to 2004 using satellite data and the CASA biogeochemical model. Burned area from 2001 2004 was derived using newly available active fire and 500 m. burned area datasets from MODIS following the approach described by Giglio et al. ( 2006). ATSR and VIRS satellite data were used to extend the burned area time series back in time through 1997. In our analysis we estimated fuel loads, including organic soil layer and peatland fuels, and the net flux from terrestrial ecosystems as the balance between net primary production (NPP), heterotrophic respiration (R-h), and biomass burning, using time varying inputs of precipitation (PPT), temperature, solar radiation, and satellite-derived fractional absorbed photosynthetically active radiation (fA-PAR). For the 1997 - 2004 period, we found that on average approximately 58 PgC year(-1) was fixed by plants as NPP, and approximately 95% of this was returned back to the atmosphere via R-h. Another 4%, or 2.5 Pg C year(-1) was emitted by biomass burning; the remainder consisted of losses from fuel wood collection and subsequent burning. At a global scale, burned area and total fire emissions were largely decoupled from year to year. Total carbon emissions tracked burning in forested areas ( including deforestation fires in the tropics), whereas burned area was largely controlled by savanna fires that responded to different environmental and human factors. Biomass burning emissions showed large interannual variability with a range of more than 1 Pg C year(-1), with a maximum in 1998 (3.2 Pg C year(-1)) and a minimum in 2000 (2.0 Pg C year(-1)). C1 Vrije Univ Amsterdam, Fac Earth & Life Sci, Dept Hydrol & Geoenvironm Sci, Amsterdam, Netherlands. Univ Calif Irvine, Dept Earth Syst Sci, Irvine, CA USA. NASA, Goddard Space Flight Ctr, Sci Syst & Applicat Inc, Greenbelt, MD 20771 USA. Duke Univ, Nicholas Sch Environm & Earth Sci, Durham, NC USA. RP van der Werf, GR (reprint author), Vrije Univ Amsterdam, Fac Earth & Life Sci, Dept Hydrol & Geoenvironm Sci, Amsterdam, Netherlands. EM guido.van.der.werf@falw.vu.nl RI Arellano, Avelino, Jr./F-5674-2010; Kasibhatla, Prasad/A-2574-2010; collatz, george/D-5381-2012; van der Werf, Guido/M-8260-2016; OI van der Werf, Guido/0000-0001-9042-8630; Kasibhatla, Prasad/0000-0003-3562-3737 NR 78 TC 851 Z9 866 U1 25 U2 232 PU COPERNICUS GESELLSCHAFT MBH PI GOTTINGEN PA BAHNHOFSALLEE 1E, GOTTINGEN, 37081, GERMANY SN 1680-7316 EI 1680-7324 J9 ATMOS CHEM PHYS JI Atmos. Chem. Phys. PD AUG 21 PY 2006 VL 6 BP 3423 EP 3441 PG 19 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 075TI UT WOS:000239907700004 ER PT J AU Dufour, G Boone, CD Rinsland, CP Bernath, PF AF Dufour, G. Boone, C. D. Rinsland, C. P. Bernath, P. F. TI First space-borne measurements of methanol inside aged southern tropical to mid-latitude biomass burning plumes using the ACE-FTS instrument SO ATMOSPHERIC CHEMISTRY AND PHYSICS LA English DT Article ID TRANSFORM INFRARED-SPECTROSCOPY; NONMETHANE HYDROCARBONS; ATMOSPHERIC CHEMISTRY; TROPOSPHERIC OZONE; TRACE GASES; EMISSIONS; FORMALDEHYDE; PARAMETERS; ATLANTIC; DATABASE AB First measurements from space of upper tropospheric and lower stratospheric methanol profiles within aged fire plumes are reported. Elevated levels of methanol at 0 -45 degrees S from 30 September to 3 November 2004 have been measured by the high resolution infrared spectrometer ACE-FTS onboard the SCISAT satellite. Methanol volume mixing ratios higher than 4000 pptv are detected and are strongly correlated with other fire products such as CO, C2H6, and HCN. A sensitivity study of the methanol retrieval, accounting for random and systematic contributions, shows that the retrieved methanol profile for a single occultation exceeds 100% error above 16.5 km, with an accuracy of about 20% for measurements inside polluted air masses. The upper tropospheric enhancement ratio of methanol with respect to CO is estimated from the correlation plot between methanol and CO for aged tropical biomass burning plumes. This ratio is in good agreement with the ratio measured in the free troposphere ( up to 12 km) by recent aircraft studies and does not suggest any secondary production of methanol by oxidation in aged biomass burning plumes. C1 Inst Pierre Simon Laplace, Meteorol Dynam Lab, Palaiseau, France. Univ Waterloo, Dept Chem, Waterloo, ON N2L 3G1, Canada. NASA, Langley Res Ctr, Hampton, VA 23665 USA. RP Dufour, G (reprint author), Inst Pierre Simon Laplace, Meteorol Dynam Lab, Palaiseau, France. EM gaelle.dufour@lmd.polytechnique.fr RI Bernath, Peter/B-6567-2012 OI Bernath, Peter/0000-0002-1255-396X NR 28 TC 25 Z9 25 U1 0 U2 0 PU EUROPEAN GEOSCIENCES UNION PI KATLENBURG-LINDAU PA MAX-PLANCK-STR 13, 37191 KATLENBURG-LINDAU, GERMANY SN 1680-7316 J9 ATMOS CHEM PHYS JI Atmos. Chem. Phys. PD AUG 21 PY 2006 VL 6 BP 3463 EP 3470 PG 8 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 075TI UT WOS:000239907700006 ER PT J AU Groner, P Herbst, E De Lucia, FC Drouin, BJ Mader, H AF Groner, Peter Herbst, Eric De Lucia, Frank C. Drouin, Brian J. Maeder, Heinrich TI Rotational spectrum of acetone, CH3COCH3, in the first torsional excited state SO JOURNAL OF MOLECULAR STRUCTURE LA English DT Article DE acetone; rotational spectroscopy; internal rotation; torsional excited state ID MICROWAVE FOURIER-TRANSFORM; INTERNAL-ROTATION; LABORATORY ASSIGNMENTS; INTERSTELLAR ACETONE; POTENTIAL FUNCTION; GROUND-STATE; GHZ; PREDICTIONS; MOLECULES; ROTORS AB The rotational spectrum of acetone in its first torsional excited state (80 cm(-1) above the ground state) has been identified and assigned. The vibrational levels of acetone are split into four torsional substates because of the interaction between overall rotation and the internal rotation motions of the two methyl groups, which results in torsional splittings of the rotational transitions. These splittings are significantly larger in the torsional excited state than in the ground vibrational state, making assignment difficult. Nevertheless, initial assignments were made between 260 and 344 GHz using Loomis-Wood diagrams. The assignment was then extended both into the 72-122 and 176-253 GHz regions and into the microwave spectral region. Eventually, 40 parameters of an effective rotational Hamiltonian for a molecule with two periodic internal motions were fit to frequencies of 571 transitions and 50 blends to near experimental precision. Preliminary results have already been used to help radio-astronomers identify vibrationally excited acetone in interstellar hot cores. (c) 2006 Elsevier B.V. All rights reserved. C1 [Groner, Peter] Univ Missouri, Dept Chem, Kansas City, MO 64110 USA. [Herbst, Eric; De Lucia, Frank C.] Ohio State Univ, Dept Phys, Columbus, OH 43210 USA. [Drouin, Brian J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Maeder, Heinrich] Univ Kiel, Inst Phys Chem, D-24098 Kiel, Germany. RP Groner, P (reprint author), Univ Missouri, Dept Chem, Kansas City, MO 64110 USA. EM gronerp@umkc.edu NR 30 TC 14 Z9 15 U1 2 U2 7 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0022-2860 EI 1872-8014 J9 J MOL STRUCT JI J. Mol. Struct. PD AUG 21 PY 2006 VL 795 IS 1-3 BP 173 EP 178 DI 10.1016/j.molstruc.2006.02.028 PG 6 WC Chemistry, Physical SC Chemistry GA 088XY UT WOS:000240845600019 ER PT J AU De Pasquale, M Grupe, D Poole, TS Breeveld, AA Zane, S Rosen, SR Page, MJ Mason, KO Burrows, DN Krimm, HA Gehrels, N Nousek, JA Roming, PWA Kobayashi, S Zhang, B AF De Pasquale, Massimiliano Grupe, Dirk Poole, T. S. Breeveld, A. A. Zane, S. Rosen, S. R. Page, M. J. Mason, K. O. Burrows, D. N. Krimm, H. A. Gehrels, N. Nousek, J. A. Roming, P. W. A. Kobayashi, S. Zhang, B. TI Swift observations of GRB 050712 SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE gamma-rays : bursts ID GAMMA-RAY BURST; AFTERGLOW; SUPERNOVA; EMISSION; TELESCOPE; LIGHT; EVOLUTION; DENSITY; ENGINE; PROBE AB We present the results of X-ray and optical observations of GRB 050712 performed by Swift. The X-ray light curve of this burst exhibits episodes of flares in the first 1000 s, the same epoch at which the UVOT detected an optical counterpart. A shallow X-ray decay, with a decay slope of alpha = -0.73, followed and lasted similar to 70 ks. This behaviour can be explained in terms of activity of the gamma-ray burst 'inner engine', with the possibility that the last flare is caused by the interaction of the ejecta with the surrounding medium. We also find interesting spectral parameters for the X-ray emission. In particular, data suggest the presence of an intrinsic absorption in the first 1000 s, which can be explained if circumburst medium clouds lie along the line of sight. C1 UCL, Mullard Space Sci Lab, Dorking RH5 6NT, Surrey, England. Penn State Univ, Dept Astron & Astrophys, Davey Lab 525, University Pk, PA 16802 USA. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Univ Space Res Assoc, Columbia, MD 21044 USA. Liverpool John Moores Univ, Astrophys Res Inst, Birkenhead CH4 1LD, Merseyside, England. Univ Nevada, Dept Phys, Las Vegas, NV 89154 USA. RP De Pasquale, M (reprint author), UCL, Mullard Space Sci Lab, Holmbury St Mary, Dorking RH5 6NT, Surrey, England. EM mdp@mssl.ucl.ac.uk RI Gehrels, Neil/D-2971-2012 NR 54 TC 10 Z9 10 U1 0 U2 1 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD AUG 21 PY 2006 VL 370 IS 4 BP 1859 EP 1866 DI 10.1111/j.1365-2966.2006.10609.x PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 070JG UT WOS:000239517300025 ER PT J AU Bautista, MA Hartman, H Gull, TR Smith, N Lodders, K AF Bautista, M. A. Hartman, H. Gull, T. R. Smith, N. Lodders, K. TI [Ti II] and [Ni II] emission from the strontium filament of eta Carinae SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE atomic data; atomic processes; line : formation; stars : abundances ID OSCILLATOR-STRENGTHS; HOMUNCULUS-NEBULA; TRANSITION-PROBABILITIES; CHEMICAL ENRICHMENT; ATOMIC STRUCTURES; IONIZED TITANIUM; FERRUM PROJECT; IRON PROJECT; ULTRAVIOLET; EJECTA AB We study the nature of the [Ti II] and [Ni II] emission from the so-called strontium filament found in the ejecta of eta Carinae. To this purpose, we employ multilevel models of the Ti II and Ni II systems, which are used to investigate the physical condition of the filament and the excitation mechanisms of the observed lines. For the Ti II ion, for which no atomic data were previously available, we carry out ab initio calculations of radiative transition rates and electron impact excitation rate coefficients. It is found that the observed spectrum is consistent with the lines being excited in a mostly neutral region with an electron density of the order of 10(7) cm(-3) and a temperature around 6000 K. In analysing three observations with different slit orientations recorded between 2000 March and 2001 November, we find line ratios that change among various observations, in a way consistent with changes of up to an order of magnitude in the strength of the continuum radiation field. These changes result from different samplings of the extended filament due to the different slit orientations used for each observation, and yield clues on the spatial extent and optical depth of the filament. The observed emission indicates a large Ti/Ni abundance ratio relative to solar abundances. It is suggested that the observed high Ti/Ni ratio in gas is caused by dust-gas fractionation processes and does not reflect the absolute Ti/Ni ratio in the ejecta of eta Carinae. We study the condensation chemistry of Ti, Ni and Fe within the filament and suggest that the observed gas phase overabundance of Ti is likely the result of selective photoevaporation of Ti-bearing grains. Some mechanisms for such a scenario are proposed. C1 Inst Venezolano Invest Cient, Ctr Fis, Caracas 1020A, Venezuela. Lund Univ, Lund Observ, SE-22100 Lund, Sweden. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Univ Colorado, Ctr Astrophys & Space Astron, Boulder, CO 80309 USA. Washington Univ, Dept Earth & Planetary Sci, Planetary Chem Lab, St Louis, MO 63130 USA. RP Bautista, MA (reprint author), Inst Venezolano Invest Cient, Ctr Fis, POB 21827, Caracas 1020A, Venezuela. EM bautista@kant.ivic.ve RI Gull, Theodore/D-2753-2012; Hartman, Henrik/K-3113-2013 OI Gull, Theodore/0000-0002-6851-5380; NR 55 TC 14 Z9 14 U1 0 U2 0 PU BLACKWELL PUBLISHING PI OXFORD PA 9600 GARSINGTON RD, OXFORD OX4 2DQ, OXON, ENGLAND SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD AUG 21 PY 2006 VL 370 IS 4 BP 1991 EP 2003 DI 10.1111/j.1365-2966.2006.10624.x PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 070JG UT WOS:000239517300038 ER PT J AU MacTavish, CJ Ade, PAR Bock, JJ Bond, JR Borrill, J Boscaleri, A Cabella, P Contaldi, CR Crill, BP De Bernardis, P De Gasperis, G De Oliveira-Costa, A De Troia, G Di Stefano, G Hivon, E Jaffe, AH Jones, WC Kisner, TS Lange, AE Lewis, AM Masi, S Mauskopf, PD Melchiorri, A Montroy, TE Natoli, P Netterfield, CB Pascale, E Piacentini, F Pogosyan, D Polenta, G Prunet, S Ricciardi, S Romeo, G Ruhl, JE Santini, P Tegmark, M Veneziani, M Vittorio, N AF MacTavish, C. J. Ade, P. A. R. Bock, J. J. Bond, J. R. Borrill, J. Boscaleri, A. Cabella, P. Contaldi, C. R. Crill, B. P. De Bernardis, P. De Gasperis, G. De Oliveira-Costa, A. De Troia, G. Di Stefano, G. Hivon, E. Jaffe, A. H. Jones, W. C. Kisner, T. S. Lange, A. E. Lewis, A. M. Masi, S. Mauskopf, P. D. Melchiorri, A. Montroy, T. E. Natoli, P. Netterfield, C. B. Pascale, E. Piacentini, F. Pogosyan, D. Polenta, G. Prunet, S. Ricciardi, S. Romeo, G. Ruhl, J. E. Santini, P. Tegmark, M. Veneziani, M. Vittorio, N. TI Cosmological parameters from the 2003 flight of BOOMERANG SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmic microwave background; cosmological parameters; polarization ID PROBE WMAP OBSERVATIONS; ANGULAR POWER SPECTRUM; MICROWAVE BACKGROUND ANISOTROPIES; GALAXY REDSHIFT SURVEY; HUBBLE-SPACE-TELESCOPE; DIGITAL SKY SURVEY; POLARIZATION; UNIVERSE; IMAGER; FLUCTUATIONS AB We present the cosmological parameters from the CMB intensity and polarization power spectra of the 2003 Antarctic flight of the BOOMERANG telescope. The BOOMERANG data alone constrain the parameters of the Lambda CDM model remarkably well and are consistent with constraints from a multiexperiment combined CMB data set. We add LSS data from the 2dF and SDSS redshift surveys to the combined CMB data set and test several extensions to the standard model including running of the spectral index, curvature, tensor modes, the effect of massive neutrinos, and an effective equation of state for dark energy. We also include an analysis of constraints to a model that allows a CDM isocurvature admixture. C1 Univ Toronto, Dept Phys, Toronto, ON M5S 1A7, Canada. Cardiff Univ, Sch Phys & Astron, Cardiff CF24 3YB, Wales. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. Univ Toronto, Canadian Inst Theoret Astrophys, Toronto, ON M5S 3H8, Canada. Univ Calif Berkeley, Lawrence Berkeley Lab, Natl Energy Res Sci Comp Ctr, Berkeley, CA 94720 USA. CNR, IFAC, I-50127 Florence, Italy. Univ Roma Tor Vergata, Dipartimento Fis, I-00133 Rome, Italy. Imperial Coll Sch Med, Dept Phys, London SW7 2BW, England. CALTECH, Ctr Infrared Proc & Anal, Pasadena, CA 91125 USA. Univ Roma La Sapienza, Dipartimento Fis, I-00185 Rome, Italy. MIT, Dept Phys, Cambridge, MA 02139 USA. Ist Nazl Geofis & Vulcanol, I-00143 Rome, Italy. CALTECH, Dept Phys, Pasadena, CA 91125 USA. Case Western Reserve Univ, Dept Phys, Cleveland, OH 44106 USA. Ist Nazl Fis Nucl, Sez Roma 1, I-00133 Rome, Italy. Ist Nazl Fis Nucl, Sez Roma 2, I-00133 Rome, Italy. Univ Toronto, Dept Astron & Astrophys, Toronto, ON M5S 3H8, Canada. Univ Alberta, Dept Phys, Edmonton, AB T6G 2J1, Canada. Inst Astrophys, F-75014 Paris, France. RP MacTavish, CJ (reprint author), Univ Toronto, Dept Phys, 60 St George St, Toronto, ON M5S 1A7, Canada. RI Jaffe, Andrew/D-3526-2009; de Gasperis, Giancarlo/C-8534-2012; Piacentini, Francesco/E-7234-2010; OI Hivon, Eric/0000-0003-1880-2733; de Gasperis, Giancarlo/0000-0003-2899-2171; Piacentini, Francesco/0000-0002-5444-9327; de Bernardis, Paolo/0000-0001-6547-6446; Masi, Silvia/0000-0001-5105-1439; ROMEO, Giovanni/0000-0002-5535-7803; Polenta, Gianluca/0000-0003-4067-9196; Ricciardi, Sara/0000-0002-3807-4043; Santini, Paola/0000-0002-9334-8705; Melchiorri, Alessandro/0000-0001-5326-6003 NR 65 TC 143 Z9 145 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD AUG 20 PY 2006 VL 647 IS 2 BP 799 EP 812 DI 10.1086/505558 PN 1 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 074RR UT WOS:000239830000007 ER PT J AU Montroy, TE Ade, PAR Bock, JJ Bond, JR Borrill, J Boscaleri, A Cabella, P Contaldi, CR Crill, BP De Bernardis, P De Gasperis, G De Oliveira-Costa, A De Troia, G Di Stefano, G Hivon, E Jaffe, AH Kisner, TS Jones, WC Lange, AE Masi, S Mauskopf, PD MacTavish, CJ Melchiorri, A Natoli, P Netterfield, CB Pascale, E Piacentini, F Pogosyan, D Polenta, G Prunet, S Ricciardi, S Romeo, G Ruhl, JE Santini, P Tegmark, M Veneziani, M Vittorio, N AF Montroy, T. E. Ade, P. A. R. Bock, J. J. Bond, J. R. Borrill, J. Boscaleri, A. Cabella, P. Contaldi, C. R. Crill, B. P. De Bernardis, P. De Gasperis, G. De Oliveira-Costa, A. De Troia, G. Di Stefano, G. Hivon, E. Jaffe, A. H. Kisner, T. S. Jones, W. C. Lange, A. E. Masi, S. Mauskopf, P. D. MacTavish, C. J. Melchiorri, A. Natoli, P. Netterfield, C. B. Pascale, E. Piacentini, F. Pogosyan, D. Polenta, G. Prunet, S. Ricciardi, S. Romeo, G. Ruhl, J. E. Santini, P. Tegmark, M. Veneziani, M. Vittorio, N. TI A measurement of the CMB {EE} spectrum from the 2003 flight of BOOMERANG SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmic microwave background; instrumentation : detectors ID MICROWAVE BACKGROUND POLARIZATION; PROBE WMAP OBSERVATIONS; ANGULAR POWER SPECTRUM; COSMOLOGICAL PARAMETERS; ANISOTROPY; RADIATION; EMISSION; TEMPERATURE; FOREGROUNDS; ARCHEOPS AB We report measurements of the CMB polarization power spectra from the 2003 January Antarctic flight of BOOMERANG. The primary results come from 6 days of observation of a patch covering 0.22% of the sky centered near R.A. = 82.degrees 5, decl. = -45 degrees. The observations were made using four pairs of polarization- sensitive bolometers operating in bands centered at 145 GHz. Using two independent analysis pipelines, we measure a nonzero < EE > signal in the range 201 < l < 1000 with a significance of 4.8 alpha, a 2 alpha upper limit of 8.6 mu K-2 for any < BB > contribution, and a 2 sigma upper limit of 7.0 mu K-2 for the < EB > spectrum. Estimates of foreground intensity fluctuations and the nondetection of < BB > and < EB > signals rule out any significant contribution from Galactic foregrounds. The results are consistent with a Lambda CDM cosmology seeded by adiabatic perturbations. We note that this is the first detection of CMB polarization with bolometric detectors. C1 Case Western Reserve Univ, Dept Phys, Cleveland, OH 44106 USA. Univ Cardiff Wales, Sch Phys & Astron, Cardiff CF24 3YB, Wales. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. CALTECH, Pasadena, CA 91125 USA. Univ Toronto, Canadian Inst Theoret Astrophys, Toronto, ON M5S 3H8, Canada. Univ Calif Berkeley, Lawrence Berkeley Lab, Div Computat Res, Berkeley, CA 94720 USA. Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. CNR, IFAC, I-50127 Florence, Italy. Univ Roma Tor Vergata, Dipartimento Fis, I-00133 Rome, Italy. Imperial Coll Sch Med, Theoret Phys Grp, London SW7 2BW, England. CALTECH, IPAC, Pasadena, CA 91125 USA. Univ Roma La Sapienza, Dipartimento Fis, I-00185 Rome, Italy. MIT, Dept Phys, Cambridge, MA 02139 USA. Ist Nazl Geofis & Vulcanol, I-00143 Rome, Italy. Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA. Univ Toronto, Dept Phys, Toronto, ON M5S 3H8, Canada. Ist Nazl Fis Nucl, Sez Roma 1, I-00133 Rome, Italy. Ist Nazl Fis Nucl, Sez Roma 2, I-00133 Rome, Italy. Univ Toronto, Dept Astron & Astrophys, Toronto, ON M5S 3H8, Canada. Univ Alberta, Dept Phys, Edmonton, AB T6G 2J1, Canada. Inst Astrophys, F-75014 Paris, France. RP Montroy, TE (reprint author), Case Western Reserve Univ, Dept Phys, 10900 Euclid Ave, Cleveland, OH 44106 USA. RI Jaffe, Andrew/D-3526-2009; de Gasperis, Giancarlo/C-8534-2012 OI de Gasperis, Giancarlo/0000-0003-2899-2171 NR 48 TC 203 Z9 203 U1 0 U2 4 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD AUG 20 PY 2006 VL 647 IS 2 BP 813 EP 822 DI 10.1086/505560 PN 1 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 074RR UT WOS:000239830000008 ER PT J AU Jones, WC Ade, PAR Bock, JJ Bond, JR Borrill, J Boscaleri, A Cabella, P Contaldi, CR Crill, BP De Bernardis, P De Gasperis, G De Oliveira-Costa, A De Troia, G Di Stefano, G Hivon, E Jaffe, AH Kisner, TS Lange, AE MacTavish, CJ Masi, S Mauskopf, PD Melchiorri, A Montroy, TE Natoli, P Netterfield, CB Pascale, E Piacentini, F Pogosyan, D Polenta, G Prunet, S Ricciardi, S Romeo, G Ruhl, JE Santini, P Tegmark, M Veneziani, M Vittorio, N AF Jones, W. C. Ade, P. A. R. Bock, J. J. Bond, J. R. Borrill, J. Boscaleri, A. Cabella, P. Contaldi, C. R. Crill, B. P. De Bernardis, P. De Gasperis, G. De Oliveira-Costa, A. De Troia, G. Di Stefano, G. Hivon, E. Jaffe, A. H. Kisner, T. S. Lange, A. E. MacTavish, C. J. Masi, S. Mauskopf, P. D. Melchiorri, A. Montroy, T. E. Natoli, P. Netterfield, C. B. Pascale, E. Piacentini, F. Pogosyan, D. Polenta, G. Prunet, S. Ricciardi, S. Romeo, G. Ruhl, J. E. Santini, P. Tegmark, M. Veneziani, M. Vittorio, N. TI A measurement of the angular power spectrum of the CMB temperature anisotropy from the 2003 flight of BOOMERANG SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmic microwave background; cosmology : observations; instrumentation : detectors ID PROBE WMAP OBSERVATIONS; MICROWAVE BACKGROUND-RADIATION; GALACTIC DUST EMISSION; MULTIPLE PEAKS; DATA SETS; POLARIZATION; MAPS; RECEIVER AB We report on observations of the cosmic microwave background ( CMB) obtained during the 2003 January flight of BOOMERANG. These results are derived from 195 hr of observation with four 145 GHz polarization- sensitive bolometer ( PSB) pairs, identical in design to the four 143 GHz Planck High Frequency Instrument ( HFI) polarized pixels. The data include 75 hr of observations distributed over 1.84% of the sky with an additional 120 hr concentrated on the central portion of the field, which represents 0.22% of the full sky. From these data we derive an estimate of the angular power spectrum of temperature fluctuations of the CMB in 24 bands over the multipole range 50 <= l <= 1500. A series of features, consistent with those expected from acoustic oscillations in the primordial photon-baryon fluid, are clearly evident in the power spectrum, as is the exponential damping of power on scales smaller than the photon mean free path at the epoch of last scattering (l greater than or similar to 900). As a consistency check, the collaboration has performed two fully independent analyses of the time-ordered data, which are found to be in excellent agreement. C1 CALTECH, Dept Phys, Pasadena, CA 91125 USA. Cardiff Univ, Sch Phys & Astron, Cardiff CF24 3YB, Wales. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. Univ Toronto, CITA, Toronto, ON M5S 3H8, Canada. Univ Calif Berkeley, Lawrence Berkeley Lab, Computat Res Div, Berkeley, CA 94720 USA. Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. CNR, IFAC, I-50127 Florence, Italy. Univ Roma Tor Vergata, Dipartimento Fis, I-00133 Rome, Italy. Imperial Coll Sch Med, Theoret Phys Grp, London SW7 2BW, England. CALTECH, IPAC, Pasadena, CA 91125 USA. Univ Roma La Sapienza, Dipartimento Fis, I-00185 Rome, Italy. MIT, Dept Phys, Cambridge, MA 02139 USA. Inst Nazl Geofis & Vulcanol, I-00143 Rome, Italy. Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA. Case Western Reserve Univ, Dept Phys, Cleveland, OH 44106 USA. Univ Toronto, Dept Phys, Toronto, ON M5S 3H8, Canada. Ist Nazl Fis Nucl, Sez Roma 1, I-00133 Rome, Italy. Ist Nazl Fis Nucl, Sez Roma 2, I-00133 Rome, Italy. Univ Toronto, Dept Astron & Astrophys, Toronto, ON M5S 3H8, Canada. Univ Alberta, Dept Phys, Edmonton, AB T6G 2J1, Canada. Inst Astrophys, F-75014 Paris, France. RP Jones, WC (reprint author), CALTECH, Dept Phys, MS 59-33,1200 E Calif Blvd, Pasadena, CA 91125 USA. EM wcj@astro.caltech.edu RI Jaffe, Andrew/D-3526-2009; de Gasperis, Giancarlo/C-8534-2012; OI de Gasperis, Giancarlo/0000-0003-2899-2171; Masi, Silvia/0000-0001-5105-1439; de Bernardis, Paolo/0000-0001-6547-6446; ROMEO, Giovanni/0000-0002-5535-7803; Polenta, Gianluca/0000-0003-4067-9196; Ricciardi, Sara/0000-0002-3807-4043; Santini, Paola/0000-0002-9334-8705; Melchiorri, Alessandro/0000-0001-5326-6003; Piacentini, Francesco/0000-0002-5444-9327; Hivon, Eric/0000-0003-1880-2733 NR 45 TC 172 Z9 172 U1 0 U2 5 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 AUG 20 PY 2006 VL 647 IS 2 BP 823 EP 832 DI 10.1086/505559 PN 1 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 074RR UT WOS:000239830000009 ER PT J AU Piacentini, F Ade, PAR Bock, JJ Bond, JR Borrill, J Boscaleri, A Cabella, P Contaldi, CR Crill, BP De Bernardis, P De Gasperis, G De Oliveira-Costa, A De Troia, G Di Stefano, G Hivon, E Jaffe, AH Kisner, TS Jones, WC Lange, AE Masi, S Mauskopf, PD MacTavish, CJ Melchiorri, A Montroy, TE Natoli, P Netterfield, CB Pascale, E Pogosyan, D Polenta, G Prunet, S Ricciardi, S Romeo, G Ruhl, JE Santini, P Tegmark, M Veneziani, M Vittorio, N AF Piacentini, F. Ade, P. A. R. Bock, J. J. Bond, J. R. Borrill, J. Boscaleri, A. Cabella, P. Contaldi, C. R. Crill, B. P. De Bernardis, P. De Gasperis, G. De Oliveira-Costa, A. De Troia, G. Di Stefano, G. Hivon, E. Jaffe, A. H. Kisner, T. S. Jones, W. C. Lange, A. E. Masi, S. Mauskopf, P. D. MacTavish, C. J. Melchiorri, A. Montroy, T. E. Natoli, P. Netterfield, C. B. Pascale, E. Pogosyan, D. Polenta, G. Prunet, S. Ricciardi, S. Romeo, G. Ruhl, J. E. Santini, P. Tegmark, M. Veneziani, M. Vittorio, N. TI A measurement of the polarization-temperature angular cross-power spectrum of the cosmic microwave background from the 2003 flight of BOOMERANG SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmic microwave background ID PROBE WMAP OBSERVATIONS; GALACTIC DUST EMISSION; COSMOLOGICAL PARAMETERS; ANISOTROPY; INFLATION; RADIATION; SKY AB We present a measurement of the polarization- temperature angular cross power spectra, < TE > and < TB >, of the cosmic microwave background. The result is based on similar to 200 hr of data from eight polarization- sensitive bolometers operating at 145 GHz during the 2003 flight of BOOMERANG. We detect a significant < TE > correlation in the l-range between 50 and 950 with a statistical significance of > 3.5 sigma. Contamination by polarized foreground emission and systematic effects are negligible in comparison with statistical uncertainties. The spectrum is consistent with previous detections and with the ``concordance model'' that assumes adiabatic initial conditions. This is the first measurement of polarization- temperature angular cross-power spectra using bolometric detectors. C1 Univ Roma La Sapienza, Dipartimento Fis, I-00185 Rome, Italy. Cardiff Univ, Dept Phys & Astron, Cardiff CF24 3YB, Wales. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. CALTECH, Pasadena, CA 91125 USA. Univ Toronto, Canadian Inst Theoret Astrophys, Toronto, ON M5S 3H8, Canada. Univ Calif Berkeley, Lawrence Berkeley Lab, Computat Res Div, Berkeley, CA 94720 USA. Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. CNR, IFAC, I-50127 Florence, Italy. Univ Roma Tor Vergata, Dipartimento Fis, I-00133 Rome, Italy. Imperial Coll Sch Med, Theoret Phys Grp, London SW7 2BW, England. CALTECH, IPAC, Pasadena, CA 91125 USA. MIT, Dept Phys, Cambridge, MA 02139 USA. Ist Nazl Geofis & Vulcanol, I-00143 Rome, Italy. Case Western Reserve Univ, Dept Phys, Cleveland, OH 44106 USA. Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA. Univ Toronto, Dept Phys, Toronto, ON M5S 3H8, Canada. Ist Nazl Fis Nucl, Sez Roma 1, I-00133 Rome, Italy. Ist Nazl Fis Nucl, Sez Roma 2, I-00133 Rome, Italy. Univ Alberta, Dept Phys, Edmonton, AB T6G 2J1, Canada. Inst Astrophys, F-75104 Paris, France. RP Piacentini, F (reprint author), Univ Roma La Sapienza, Dipartimento Fis, Piazzale Aldo Moro 2, I-00185 Rome, Italy. RI Jaffe, Andrew/D-3526-2009; de Gasperis, Giancarlo/C-8534-2012; Piacentini, Francesco/E-7234-2010; OI Hivon, Eric/0000-0003-1880-2733; Santini, Paola/0000-0002-9334-8705; de Gasperis, Giancarlo/0000-0003-2899-2171; Piacentini, Francesco/0000-0002-5444-9327; Masi, Silvia/0000-0001-5105-1439; de Bernardis, Paolo/0000-0001-6547-6446; ROMEO, Giovanni/0000-0002-5535-7803; Polenta, Gianluca/0000-0003-4067-9196; Ricciardi, Sara/0000-0002-3807-4043; Melchiorri, Alessandro/0000-0001-5326-6003 NR 39 TC 123 Z9 123 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 AUG 20 PY 2006 VL 647 IS 2 BP 833 EP 839 DI 10.1086/505557 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 074RR UT WOS:000239830000010 ER PT J AU Swartz, DA Yukita, M Tennant, AF Soria, R Ghosh, KK AF Swartz, Douglas A. Yukita, Mihoko Tennant, Allyn F. Soria, Roberto Ghosh, Kajal K. TI Chandra observations of circumnuclear star formation in NGC 3351 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : individual (NGC 3351); galaxies : starburst; galaxies : structure; X-rays : galaxies ID X-RAY EMISSION; BLACK-HOLE; HOT GAS; STARBURST GALAXIES; DISK GALAXIES; MOLECULAR GAS; H-ALPHA; BULGES; HALOS; MASS AB The nearby SB(r)b galaxy NGC 3351 (M95) displays an similar to 600 pc diameter star-forming circumnuclear ring fueled by gas accreted through a stellar bar. The X-ray emission from this region is composed of numerous pointlike sources embedded in hot (kT = 0.5 +/- 0.1 keV), nonuniform diffuse gas. Most of the pointlike sources are likely themselves concentrated regions of hot gas. The morphology of the X-ray emission is similar to, but not identical with, UV and H alpha hot spots in the circumnuclear ring. The emission morphology can be understood if star formation is occurring through a series of instantaneous starbursts at various locations around the ring and the UV, H alpha, and X-ray emission trace successively later stages in the evolution of the underlying stellar populations. X-ray emission extends at least 500 pc beyond the circumnuclear ring. This emission is interpreted as the result of gas outflow from the star-forming ring into the disk and halo of NGC 3351. There is evidence that the outflow is confined by cold ambient gas near the plane of the galaxy but that flow out of the plane is not restricted. The nucleus of the galaxy lacks both large amounts of hot gas and any pointlike source above an estimated X-ray luminosity of 10(37) ergs s(-1) in the 0.5-8.0 keV band. This luminosity is orders of magnitude too low to account for the observed nuclear H alpha luminosity, 3.5 X 10(38) ergs s(-1), by X-ray photoionization. C1 NASA, George C Marshall Space Flight Ctr, Univ Space Res Assoc, Huntsville, AL 35805 USA. Univ Alabama, Dept Phys, Huntsville, AL 35899 USA. NASA, George C Marshall Space Flight Ctr, Dept Space Sci, Huntsville, AL 35805 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Swartz, DA (reprint author), NASA, George C Marshall Space Flight Ctr, Univ Space Res Assoc, XD12, Huntsville, AL 35805 USA. RI Yukita, Mihoko/E-4135-2017 NR 41 TC 9 Z9 9 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 AUG 20 PY 2006 VL 647 IS 2 BP 1030 EP 1039 DI 10.1086/504680 PN 1 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 074RR UT WOS:000239830000025 ER PT J AU Croft, S Van Breugel, W De Vries, W Dopita, M Martin, C Morganti, R Neff, S Oosterloo, T Schiminovich, D Stanford, SA Van Gorkom, J AF Croft, Steve Van Breugel, Wil De Vries, Wim Dopita, Mike Martin, Chris Morganti, Raffaella Neff, Susan Oosterloo, Tom Schiminovich, David Stanford, S. A. Van Gorkom, Jacqueline TI Minkowski's Object: A starburst triggered by a radio jet, revisited SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : jets; galaxies : starburst; stars : formation ID INDUCED STAR-FORMATION; SPACE-TELESCOPE OBSERVATIONS; GALAXY-EVOLUTION-EXPLORER; CENTAURUS-A; PARTICLE-ACCELERATION; DYNAMICAL MODELS; COOLING FLOWS; HIGH-REDSHIFT; 4C 41.17; EMISSION AB We present neutral hydrogen, ultraviolet, optical, and near-infrared imaging, and optical spectroscopy, of Minkowski's Object (MO), a star-forming peculiar galaxy near NGC 541. The observations strengthen evidence that star formation in MO was triggered by the radio jet from NGC 541. Key new results are the discovery of a 4.9 X 10(8) M-circle dot double H I cloud straddling the radio jet downstream from MO, where the jet changes direction and decollimates; strong detections of MO, also showing double structure, in UV and H alpha; and numerous H II regions and associated clusters in MO. In UV, MO resembles the radio-aligned, rest-frame UV morphologies in many high-redshift radio galaxies (HzRGs), also thought to be caused by jet-induced star formation. MO's stellar population is dominated by a 7.5 Myr old, 1.9 X 10(7) M-circle dot instantaneous burst, with a current star formation rate of 0.52 M-circle dot yr(-1) (concentrated upstream from where the H I column density is high). This is unlike the jet-induced star formation in Centaurus A, where the jet interacts with preexisting cold gas; in MO, the H I may have cooled out of a warmer, clumpy intergalactic or interstellar medium as a result of jet interaction, followed by the collapse of the cooling clouds and subsequent star formation (consistent with numerical simulations). Since the radio source that triggered star formation in MO is much less luminous, and therefore more common than powerful HzRGs, and because the environment around MO is not particularly special in terms of abundant dense, cold gas, jet-induced star formation in the early universe might be even more prevalent than previously thought. C1 Lawrence Livermore Natl Lab, Inst Geophys & Planetary Phys, Livermore, CA 94550 USA. Univ Calif Merced, Merced, CA 95344 USA. Univ Calif Davis, Davis, CA 95616 USA. Australian Natl Univ, Res Sch Astron & Astrophys, Weston, ACT 2611, Australia. CALTECH, Pasadena, CA 91125 USA. Netherlands Fdn Res Astron, NL-7990 AA Dwingeloo, Netherlands. Univ Groningen, Kapteyn Astron Inst, NL-9700 AV Groningen, Netherlands. NASA, Goddard Space Flight Ctr, Astron & Solar Phys Lab, Greenbelt, MD 20771 USA. Columbia Univ, Dept Astron, New York, NY 10027 USA. RP Croft, S (reprint author), Lawrence Livermore Natl Lab, Inst Geophys & Planetary Phys, L-413,700 East Ave, Livermore, CA 94550 USA. EM scroft@igpp.ucllnl.org RI Dopita, Michael/P-5413-2014; OI Dopita, Michael/0000-0003-0922-4986; Croft, Steve/0000-0003-4823-129X NR 63 TC 74 Z9 74 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD AUG 20 PY 2006 VL 647 IS 2 BP 1040 EP 1055 DI 10.1086/505526 PN 1 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 074RR UT WOS:000239830000026 ER PT J AU Linsky, JL Draine, BT Moos, HW Jenkins, EB Wood, BE Oliveira, C Blair, WP Friedman, SD Gry, C Knauth, D Kruk, JW Lacour, S Lehner, N Redfield, S Shull, JM Sonneborn, G Williger, GM AF Linsky, Jeffrey L. Draine, Bruce T. Moos, H. W. Jenkins, Edward B. Wood, Brian E. Oliveira, Cristina Blair, William P. Friedman, Scott D. Gry, Cecile Knauth, David Kruk, Jeffrey W. Lacour, Sylvestre Lehner, Nicolas Redfield, Seth Shull, J. Michael Sonneborn, George Williger, Gerard M. TI What is the total deuterium abundance in the local galactic disk? SO ASTROPHYSICAL JOURNAL LA English DT Review DE galaxy : abundances; ISM : abundances; ISM : structure; solar neighborhood; ultraviolet : ISM ID ULTRAVIOLET-SPECTROSCOPIC-EXPLORER; ABSORPTION PROFILE SPECTROGRAPH; HUBBLE-SPACE-TELESCOPE; INTERSTELLAR MOLECULAR-HYDROGEN; BIG-BANG NUCLEOSYNTHESIS; BETA-CANIS-MAJORIS; FUSE MISSION; MILKY-WAY; COSMOLOGICAL PARAMETERS; COPERNICUS OBSERVATIONS AB Analyses of spectra obtained with the Far Ultraviolet Spectroscopic Explorer (FUSE) satellite, together with spectra from the Copernicus and interstellar medium absorption profile spectrograph (IMAPS) instruments, reveal an unexplained, very wide range in the observed deuterium/hydrogen (D/H) ratios for interstellar gas in the Galactic disk beyond the Local Bubble. We argue that spatial variations in the depletion of deuterium onto dust grains can explain these local variations in the observed gas-phase D/H ratios. We present a variable deuterium depletion model that naturally explains the constant measured values of D/H inside the Local Bubble, the wide range of gas-phase D/H ratios observed in the intermediate regime [log N(H I) = 19.2-20.7], and the low gas-phase D/H ratios observed at larger hydrogen column densities. We consider empirical tests of the deuterium depletion hypothesis: ( 1) correlations of gas-phase D/H ratios with depletions of the refractory metals iron and silicon, and (2) correlation with the H-2 rotational temperature. Both of these tests are consistent with deuterium depletion from the gas phase in cold, not recently shocked regions of the ISM, and high gas-phase D/H ratios in gas that has been shocked or otherwise heated recently. We argue that the most representative value for the total (gas plus dust) D/H ratio within 1 kpc of the Sun is >= 23.1 +/- 2.4(1 sigma) parts per million (ppm). This ratio constrains Galactic chemical evolution models to have a very small deuterium astration factor, the ratio of primordial to total (D/H) ratio in the local region of the Galactic disk, which we estimate to be f(d) <= 1.19(-0.15)(+0.16)(1 sigma) or <= 1.12 +/- 0.14(1 sigma) depending on the adopted light-element nuclear reaction rates. C1 Univ Colorado, Joint Inst Lab Astrophys, Boulder, CO 80309 USA. Natl Inst Stand & Technol, Boulder, CO 80309 USA. Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. Space Telescope Sci Inst, Baltimore, MD 21218 USA. Astrophys Lab, F-13376 Marseille, France. Northwestern Univ, Dept Phys & Astron, Evanston, IL 60208 USA. Observ Paris, LESIA, F-92195 Meudon, France. Univ Wisconsin, Dept Astron, Madison, WI 53706 USA. Univ Texas, McDonald Observ, Austin, TX 78712 USA. Univ Colorado, Ctr Astrophys & Space Astron, Dept Astrophys & Planetary Sci, Boulder, CO 80309 USA. NASA, Goddard Space Flight Ctr, Lab Observ Cosmol, Greenbelt, MD 20771 USA. RP Linsky, JL (reprint author), Univ Colorado, Joint Inst Lab Astrophys, Boulder, CO 80309 USA. EM jlinsky@jila.colorado.edu RI Sonneborn, George/D-5255-2012; Kruk, Jeffrey/G-4047-2012; Jenkins, Edward/P-5684-2014; OI Jenkins, Edward/0000-0003-1892-4423; Draine, Bruce/0000-0002-0846-936X; Redfield, Seth/0000-0003-3786-3486 NR 127 TC 159 Z9 159 U1 0 U2 6 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD AUG 20 PY 2006 VL 647 IS 2 BP 1106 EP 1124 DI 10.1086/505556 PN 1 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 074RR UT WOS:000239830000032 ER PT J AU O'Brien, PT Willingale, R Osborne, J Goad, MR Page, KL Vaughan, S Rol, E Beardmore, A Godet, O Hurkett, CP Wells, A Zhang, B Kobayashi, S Burrows, DN Nousek, JA Kennea, JA Falcone, A Grupe, D Gehrels, N Barthelmy, S Cannizzo, J Cummings, J Hill, JE Krimm, H Chincarini, G Tagliaferri, G Campana, S Moretti, A Giommi, P Perri, M Mangano, V LaParola, V AF O'Brien, P. T. Willingale, R. Osborne, J. Goad, M. R. Page, K. L. Vaughan, S. Rol, E. Beardmore, A. Godet, O. Hurkett, C. P. Wells, A. Zhang, B. Kobayashi, S. Burrows, D. N. Nousek, J. A. Kennea, J. A. Falcone, A. Grupe, D. Gehrels, N. Barthelmy, S. Cannizzo, J. Cummings, J. Hill, J. E. Krimm, H. Chincarini, G. Tagliaferri, G. Campana, S. Moretti, A. Giommi, P. Perri, M. Mangano, V. LaParola, V. TI The early X-ray emission from GRBs SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; black hole physics; gamma rays : bursts ID STANDARD ENERGY RESERVOIR; GAMMA-RAY; SWIFT OBSERVATIONS; BURST AFTERGLOWS; TELESCOPE OBSERVATIONS; STAR-FORMATION; BRIGHT; GALAXY; GRB-050709; INJECTION AB We present observations of the early X-ray emission for a sample of 40 gamma-ray bursts (GRBs) obtained using the Swift satellite, for which the narrow-field instruments were pointed at the burst within 10 minutes of the trigger. Using data from the Burst Alert Telescope and the X-Ray Telescope, we show that the X-ray light curve can be well described by an exponential that relaxes into a power law, often with flares superimposed. The transition time between the exponential and the power law provides a physically defined timescale for the burst duration. In most bursts, the power law breaks to a shallower decay within the first hour, and a late emission "hump'' is observed, which can last for many hours. In other GRBs the hump is weak or absent. The observed variety in the shape of the early X-ray light curve can be explained as a combination of three components: prompt emission from the central engine, afterglow, and the late hump. In this scenario, afterglow emission begins during or soon after the burst, and the observed shape of the X-ray light curve depends on the relative strengths of the emission due to the central engine and that of the afterglow. There is a strong correlation such that those GRBs with stronger afterglow components have brighter early optical emission. The late emission hump can have a total fluence equivalent to that of the prompt phase. GRBs with the strongest late humps have weak or no X-ray flares. C1 Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England. Univ Nevada, Dept Phys, Las Vegas, NV 89154 USA. Liverpool John Moores Univ, Astrophys Res Inst, Birkenhead CH41 1LD, Merseyside, England. Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Univ Maryland Baltimore Cty, Joint Ctr Astrophys, Baltimore, MD 21250 USA. CNR, Washington, DC 20418 USA. Univ Space Res Assoc, Columbia, MD 21044 USA. Osserv Astron Brera, INAF, I-23807 Merate, LC, Italy. Univ Milan, Dipartimento Fis, I-20126 Milan, Italy. ASI Sci Data Ctr, I-00044 Frascati, Italy. INAF, Ist Astrofis Spaziale & Fis Cosm, Sez Palermo, I-90146 Palermo, Italy. RP Page, KL (reprint author), Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England. RI Barthelmy, Scott/D-2943-2012; Gehrels, Neil/D-2971-2012; OI giommi, paolo/0000-0002-2265-5003; Perri, Matteo/0000-0003-3613-4409; La Parola, Valentina/0000-0002-8087-6488; Tagliaferri, Gianpiero/0000-0003-0121-0723 NR 72 TC 296 Z9 299 U1 0 U2 7 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD AUG 20 PY 2006 VL 647 IS 2 BP 1213 EP 1237 DI 10.1086/505457 PN 1 PG 25 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 074RR UT WOS:000239830000041 ER PT J AU Evans, NR Massa, D Fullerton, A Sonneborn, G Iping, R AF Evans, Nancy Remage Massa, Derck Fullerton, Alexander Sonneborn, George Iping, Rosina TI Cepheid masses: FUSE observations of S Muscae SO ASTROPHYSICAL JOURNAL LA English DT Article DE Cepheids; stars : fundamental parameters ID MODELS; STARS; EXTINCTION AB S Mus is the Cepheid with the hottest known companion. The large ultraviolet flux means that it is the only Cepheid companion for which the velocity amplitude could be measured with the echelle mode of the HST GHRS. Unfortunately, the high temperature is difficult to constrain at wavelengths longer than 1200 8 because of the degeneracy between temperature and reddening. We have obtained a FUSE spectrum in order to improve the determination of the temperature of the companion. Two regions that are temperature sensitive near 16,000 K but relatively unaffected by H-2 absorption (940 8 and the Ly beta wings) have been identified. By comparing FUSE spectra of S Mus B with spectra of standard stars, we have determined a temperature of 17; 000 +/- 500 K. The resulting Cepheid mass is 6: 0 +/- 0: 4 M-circle dot. This mass is consistent with main-sequence evolutionary tracks with a moderate amount of convective overshoot. C1 Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. NASA, Goddard Space Flight Ctr, SGT Inc, Greenbelt, MD 20771 USA. Univ Victoria, Dept Phys & Astron, Stn CSC, Victoria, BC V8W 3P6, Canada. RP Evans, NR (reprint author), Smithsonian Astrophys Observ, 60 Garden St,MS-4, Cambridge, MA 02138 USA. RI Sonneborn, George/D-5255-2012 NR 18 TC 16 Z9 16 U1 0 U2 3 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD AUG 20 PY 2006 VL 647 IS 2 BP 1387 EP 1392 DI 10.1086/505519 PN 1 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 074RR UT WOS:000239830000054 ER PT J AU Marengo, M Megeath, ST Fazio, GG Stapelfeldt, KR Werner, MW Backman, DE AF Marengo, M. Megeath, S. T. Fazio, G. G. Stapelfeldt, K. R. Werner, M. W. Backman, D. E. TI A Spitzer IRAC search for substellar companions of the debris disk star epsilon Eridani SO ASTROPHYSICAL JOURNAL LA English DT Article DE circumstellar matter; infrared : stars; planetary systems; stars : individual (epsilon Eridani) ID INFRARED ARRAY CAMERA; SPACE-TELESCOPE; EXTRASOLAR PLANET; GIANT PLANETS; BROWN DWARFS; DUST; VEGA; EMISSION; ROTATION; PERIOD AB We have used the Infrared Array Camera (IRAC) on board the Spitzer Space Telescope to search for low-mass companions of the nearby debris disk star is an element of Eri. The star was observed in two epochs 39 days apart, with different focal plane rotation to allow the subtraction of the instrumental point-spread function, achieving a maximum sensitivity of 0.01 MJy sr(-1) at 3.6 and 4.5 mu m, and 0.05 MJy sr(-1) at 5.8 and 8.0 mu m. This sensitivity is not sufficient to directly detect scattered or thermal radiation from the is an element of Eri debris disk. It is, however, sufficient to allow the detection of Jovian planets with mass as low as 1M(J) in the IRAC 4.5 mu m band. In this band, we detected over 460 sources within the 5'70 field of view of our images. To test if any of these sources could be a low-mass companion to is an element of Eri, we have compared their colors and magnitudes with models and photometry of low-mass objects. Of the sources detected in at least two IRAC bands, none fall into the range of mid-IR color and luminosity expected for cool, 1 Gyr substellar and planetary mass companions of is an element of Eri, as determined by both models and observations of field M, L, and T dwarfs. We identify three new sources that have detections at 4.5 mu m only, the lower limit placed on their [3.6]-[4.5] color consistent with models of planetary mass objects. Their nature cannot be established with the currently available data, and a new observation at a later epoch will be needed to measure their proper motion in order to determine if they are physically associated to is an element of Eri. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Marengo, M (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM mmarengo@cfa.harvard.edu RI Stapelfeldt, Karl/D-2721-2012 NR 44 TC 32 Z9 32 U1 0 U2 4 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD AUG 20 PY 2006 VL 647 IS 2 BP 1437 EP 1451 DI 10.1086/505531 PN 1 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 074RR UT WOS:000239830000059 ER PT J AU Phillips, KJH Chifor, C Dennis, BR AF Phillips, K. J. H. Chifor, C. Dennis, B. R. TI RHESSI observations of the solar flare iron-line feature at 6.7 keV SO ASTROPHYSICAL JOURNAL LA English DT Article DE Sun : abundances; Sun : corona; Sun : flares; Sun : X-rays, gamma rays ID X-RAY-SPECTRUM; IONIZATION BALANCE; ABUNDANCES; SPECTROMETER; ATMOSPHERES; IONS; SUN AB Analysis of RHESSI 3-10 keV spectra for 27 solar flares is reported. This energy range includes thermal free-free and free-bound continua and two line features, at similar to 6.7 and similar to 8 keV, principally due to highly ionized iron ( Fe). We used the continuum and the flux in the so-called Fe-line feature at similar to 6.7 keV to derive the electron temperature Te, the emission measure, and the Fe-line equivalent width as functions of time in each flare. The Fe/ H abundance ratio in each flare is derived from the Fe- line equivalent width as a function of Te. To minimize instrumental problems with high count rates and effects associated with multitemperature and nonthermal spectral components, spectra are presented mostly during the flare decay phase, when the emission measure and temperature were smoothly varying. We found flare Fe/ H abundance ratios that are consistent with the coronal abundance of Fe (i.e., 4 times the photospheric abundance) to within 20% for at least 17 of the 27 flares; for 7 flares, the Fe/ H abundance ratio is possibly higher by up to a factor of 2. We find evidence that the Fe xxv ion fractions are less than the theoretically predicted values by up to 60% at T-e 12 MK; the observed N(Fe xxv)/N(Fe) values appear to be displaced from the most recent theoretical values by between 1 and 3 MK. C1 NASA, Goddard Space Flight Ctr, Natl Res Council, Greenbelt, MD 20771 USA. Ctr Math Sci, Dept Appl Math & Theoret Phys, Cambridge CB3 0WA, England. RP Phillips, KJH (reprint author), Mullard Space Sci Lab, Holmbury St Mary, Dorking RH5 6NT, Surrey, England. EM kjhp@mssl.ucl.ac.uk RI Dennis, Brian/C-9511-2012 NR 24 TC 29 Z9 29 U1 0 U2 4 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD AUG 20 PY 2006 VL 647 IS 2 BP 1480 EP 1490 DI 10.1086/505518 PN 1 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 074RR UT WOS:000239830000063 ER PT J AU Monnier, JD Barry, RK Traub, WA Lane, BF Akeson, RL Ragland, S Schuller, PA Le Coroller, H Berger, JP Millan-Gabet, R Pedretti, E Schloerb, FP Koresko, C Carleton, NP Lacasse, MG Kern, P Malbet, F Perraut, K Kuchner, MJ Muterspaugh, MW AF Monnier, J. D. Barry, R. K. Traub, W. A. Lane, B. F. Akeson, R. L. Ragland, S. Schuller, P. A. Le Coroller, H. Berger, J. -P. Millan-Gabet, R. Pedretti, E. Schloerb, F. P. Koresko, C. Carleton, N. P. Lacasse, M. G. Kern, P. Malbet, F. Perraut, K. Kuchner, M. J. Muterspaugh, M. W. TI No expanding fireball: Resolving the recurrent nova RS Ophiuchi with infrared interferometry SO ASTROPHYSICAL JOURNAL LA English DT Article DE infrared : stars; novae, cataclysmic variables; stars : individual (RS Ophiuchi); techniques : interferometric ID PALOMAR TESTBED INTERFEROMETER; KECK INTERFEROMETER; 1985 OUTBURST; STARS; SYSTEMS; IOTA AB Following the recent outburst of the recurrent nova RS Oph on 2006 February 12, we measured its near-infrared size using the IOTA, Keck, and PTI Interferometers at multiple epochs. The characteristic size of similar to 3 mas hardly changed over the first 60 days of the outburst, ruling out currently popular models whereby the near-infrared emission arises from hot gas in the expanding shock. The emission was also found to be significantly asymmetric, evidenced by nonzero closure phases detected by IOTA. The physical interpretation of these data depends strongly on the adopted distance to RS Oph. Our data can be interpreted as the first direct detection of the underlying RS Oph binary, lending support to the recent "reborn red giant" models of Hachisu & Kato. However, this result hinges on an RS Oph distance of <= 540 pc, in strong disagreement with the widely adopted distance of similar to 1.6 kpc. At the farther distance, our observations imply instead the existence of a nonexpanding, dense, and ionized circumbinary gaseous disk or reservoir responsible for the bulk of the near-infrared emission. Longer baseline infrared interferometry is uniquely suited to distinguish between these models and to ultimately determine the distance, binary orbit, and component masses for RS Oph, one of the closest known (candidate) Type 1a supernova progenitor systems. C1 Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. Johns Hopkins Univ, Baltimore, MD 21218 USA. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. MIT, Cambridge, MA 02139 USA. CALTECH, Michelson Sci Ctr, Pasadena, CA 91125 USA. Calif Assoc Res Astron, WM Keck Observ, Kamuela, HI 96743 USA. Observ Haute Provence, CNRS, OAMP, F-04870 St Michel, France. Univ Grenoble 1, CNRS, Lab Astrophys Grenoble, F-38041 Grenoble, France. Univ Massachusetts, Amherst, MA 01003 USA. RP Monnier, JD (reprint author), Univ Michigan, Dept Astron, 941 Dennison Bldg, Ann Arbor, MI 48109 USA. EM monnier@umich.edu RI Kuchner, Marc/E-2288-2012 NR 28 TC 29 Z9 29 U1 0 U2 4 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD AUG 20 PY 2006 VL 647 IS 2 BP L127 EP L130 DI 10.1086/507584 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 074RV UT WOS:000239830400011 ER PT J AU Murashima, M Kokubun, M Makishima, K Kotoku, J Murakami, H Matsushita, K Hayashida, K Arnaud, K Hamaguchi, K Matsumoto, H AF Murashima, M. Kokubun, M. Makishima, K. Kotoku, J. Murakami, H. Matsushita, K. Hayashida, K. Arnaud, K. Hamaguchi, K. Matsumoto, H. TI Suzaku reveals helium-burning products in the X-ray-emitting planetary nebula BD+30 3639 SO ASTROPHYSICAL JOURNAL LA English DT Article DE planetary nebulae : general; planetary nebulae : individual (BD+30 3639); X-rays : ISM ID WC CENTRAL STARS; ONBOARD ASTRO-E2; EMISSION; BD+30-DEGREES-3639; ABUNDANCES; DISTANCES; EVOLUTION; CHANDRA AB BD + 30 3639, the brightest planetary nebula at X-ray energies, was observed with Suzaku, an X-ray observatory launched on 2005 July 10. Using the X-ray Imaging Spectrometer, the K lines from C VI, O VII, and O VIII were resolved for the first time, and the C/O, N/O, and Ne/O abundance ratios were determined. The C/O and Ne/O abundance ratios exceed the solar value by factors of at least 30 and 5, respectively. These results indicate that the X-rays are emitted mainly by helium-shell-burning products. C1 Univ Tokyo, Dept Phys, Bunkyo Ku, Tokyo 1130011, Japan. Inst Phys & Chem Res, Wako, Saitama 3510198, Japan. Tokyo Inst Technol, Dept Phys, Meguro Ku, Tokyo 1528551, Japan. Inst Space & Astronaut Sci, PLAIN Ctr, JAXA, Sagamihara, Kanagawa 2298510, Japan. Tokyo Univ Sci, Fac Sci, Dept Phys, Shinjuku Ku, Tokyo 1628601, Japan. Osaka Univ, Dept Earth & Space Sci, Toyonaka, Osaka 5600043, Japan. NASA, Goddard Space Flight Ctr, Explorat Universe Div, Greenbelt, MD 20771 USA. Kyoto Univ, Dept Phys, Sakyo Ku, Kyoto 6068502, Japan. RP Murashima, M (reprint author), Univ Tokyo, Dept Phys, Bunkyo Ku, 7-3-1 Hongo, Tokyo 1130011, Japan. RI XRAY, SUZAKU/A-1808-2009 NR 22 TC 9 Z9 9 U1 0 U2 2 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD AUG 20 PY 2006 VL 647 IS 2 BP L131 EP L134 DI 10.1086/507465 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 074RV UT WOS:000239830400012 ER PT J AU Schwartz, DA Marshall, HL Lovell, JEJ Murphy, DW Bicknell, GV Birkinshaw, M Gelbord, JM Georganopoulos, M Godfrey, L Jauncey, DL Jester, S Perlman, ES Worrall, DM AF Schwartz, D. A. Marshall, H. L. Lovell, J. E. J. Murphy, D. W. Bicknell, G. V. Birkinshaw, M. Gelbord, J. M. Georganopoulos, M. Godfrey, L. Jauncey, D. L. Jester, S. Perlman, E. S. Worrall, D. M. TI Discovery of an X-ray jet and extended jet structure in the quasar PKS 1055+201 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : jets; quasars : general; quasars : individual (PKS 1055+201, 4C 20.24); X-rays : galaxies ID ACTIVE GALACTIC NUCLEI; RADIO-SOURCES AB This Letter reports rich X-ray jet structures found in the Chandra observation of PKS 1055 +/- 201. In addition to an X-ray jet coincident with the radio jet, we detect a region of extended X-ray emission surrounding the jet as far from the core as the radio hot spot to the north, and a similar extended X-ray region along the presumed path of the unseen counterjet to the southern radio lobe. Both X-ray regions show a similar curvature to the west, relative to the quasar. We interpret this as the first example in which we separately detect the X-ray emission from a narrow jet and extended, residual jet plasma over the entire length of a powerful FR II jet. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. CSIRO, Australia Telescope Natl Facil, Epping, NSW 1710, Australia. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. Australian Natl Univ, Res Sch Astron & Astrophys, Canberra, ACT 72611, Australia. Univ Bristol, Dept Phys, Bristol BS8 1TL, Avon, England. Univ Maryland Baltimore Cty, Dept Phys, Joint Ctr Astrophys, Baltimore, MD 21250 USA. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England. RP Schwartz, DA (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM das@head-cfa.harvard.edu; hermanm@space.mit.edu; jonathan@space.mit.edu; dwm@sgra.jpl.nasa.gov; geoff@mso.anu.edu.au; mark.birkinshaw@bristol.ac.uk; markos@jca.umbc.edu; lgodfrey@mso.anu.edu.au; djauncey@atnf.csiro.au; jester@phys.soton.ac.uk; perlman@jca.umbc.edu; d.worrall@bristol.ac.uk RI Godfrey, Leith/B-5283-2013 NR 19 TC 9 Z9 9 U1 0 U2 3 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD AUG 20 PY 2006 VL 647 IS 2 BP L107 EP L110 DI 10.1086/507529 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 074RV UT WOS:000239830400006 ER PT J AU Vuitton, V Yelle, RV Anicich, VG AF Vuitton, V. Yelle, R. V. Anicich, V. G. TI The nitrogen chemistry of Titan's upper atmosphere revealed SO ASTROPHYSICAL JOURNAL LA English DT Article DE astrochemistry; planets and satellites : individual (Titan) ID GAS-PHASE; HETERODYNE OBSERVATIONS; ION CHEMISTRY; IONOSPHERE; AEROSOLS; PHOTOCHEMISTRY; MILLIMETER; SIMULATION; MOLECULES; PLASMA AB Titan's atmosphere is unique because dissociation of N-2 and CH4, the primary atmospheric constituents, provides the H, C, and N atoms necessary for the synthesis of complex organic molecules. The first steps in the synthesis of organic molecules occur in the upper atmosphere where energetic photons and electrons dissociate N-2 and CH4. We determine the abundance of a suite of nitrogen- bearing molecules in Titan's upper atmosphere through analysis of measurements of the ionospheric composition made by the Ion Neutral Mass Spectrometer (INMS) on the Cassini spacecraft. We show that the density of ions in Titan's upper atmosphere depends closely on the composition of the neutral atmosphere and that, for many species, measurement of associated ions coupled with simple chemical models provides the most sensitive determination of their abundance. With this technique we determine the densities of C 2 H 4, C4H2, HCN, HC3N, CH3CN, NH3, C2H3CN, C2H5CN, and CH2NH. The latter four species have not previously been detected in the gas phase on Titan, and none of these species have been accurately measured in the upper atmosphere. The presence of these species implies that nitrogen chemistry on Titan is more extensive than previously realized. C1 Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA. Jet Prop Lab, Pasadena, CA 91040 USA. RP Vuitton, V (reprint author), Univ Arizona, Lunar & Planetary Lab, 1629 E Univ Blvd, Tucson, AZ 85721 USA. EM vvuitton@lpl.arizona.edu; yelle@lpl.arizona.edu; vanicich@verizon.net NR 29 TC 129 Z9 129 U1 0 U2 27 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD AUG 20 PY 2006 VL 647 IS 2 BP L175 EP L178 DI 10.1086/507467 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 074RV UT WOS:000239830400023 ER PT J AU Ybarra, JE Barsony, M Haisch, KE Jarrett, TH Sahai, R Weinberger, AJ AF Ybarra, Jason E. Barsony, Mary Haisch, Karl E., Jr. Jarrett, Thomas H. Sahai, Raghvendra Weinberger, Alycia J. TI First evidence of a precessing jet excavating a protostellar envelope SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM : jets and outflows; stars : formation; stars : individual (Elias 29) ID MOLECULAR OUTFLOWS DRIVEN; YOUNG STELLAR OBJECTS; STAR-FORMING REGIONS; HYDRODYNAMIC SIMULATIONS; INFRARED OBSERVATIONS; IMAGING SURVEY; PROTOSTARS; OPHIUCHUS; TAURUS; MULTIPLICITY AB We present new, sensitive, near-infrared images of the Class I protostar, Elias 29, in the Ophiuchus cloud core. To explore the relationship between the infall envelope and the outflow, narrowband H-2 1-0 S(1), Br gamma, and K-cont filters were used to image the source with the Wide-Field Infrared Camera on the Hale 5 m telescope and with Persson's Auxiliary Nasmyth Infrared Camera on the Baade 6.5 m telescope. The source appears as a bipolar, scattered light nebula, with a wide opening angle in all filters, as is typical for late-stage protostars. However, the pure emission-line images point to the presence of a heretofore undetected precessing jet. It is argued that high-velocity, narrow, precessing jets provide the mechanism for creating the observed wide-angled outflow cavity in this source. C1 San Francisco State Univ, Dept Phys & Astron, San Francisco, CA 94132 USA. Utah Valley State Coll, Orem, UT 84058 USA. CALTECH, Ctr Infrared Proc & Anal, Pasadena, CA 91125 USA. Jet Prop Lab, Pasadena, CA 91109 USA. Space Sci Inst, Boulder, CO 80301 USA. RP Ybarra, JE (reprint author), San Francisco State Univ, Dept Phys & Astron, 1600 Holloway Dr, San Francisco, CA 94132 USA. EM jybarra@stars.sfsu.edu; mbarsony@stars.sfsu.edu; haischka@uvsc.edu; jarrett@ipac.caltech.edu; Raghvendra.Sahai@jpl.nasa.gov; weinberger@dtm.ciw.edu OI Ybarra, Jason/0000-0002-3576-4508; Weinberger, Alycia/0000-0001-6654-7859 NR 38 TC 17 Z9 17 U1 1 U2 4 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD AUG 20 PY 2006 VL 647 IS 2 BP L159 EP L162 DI 10.1086/507449 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 074RV UT WOS:000239830400019 ER PT J AU Atlas, D Ulbrich, C AF Atlas, David Ulbrich, Carlton TI Drop size spectra and integral remote sensing parameters in the transition from convective to stratiform rain SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID MICROPHYSICAL STRUCTURE; RADAR OBSERVATIONS; DISTRIBUTIONS; DISDROMETER; CLOUDS; MODEL; SHAPE AB Several authors have reported the correlation between the shape (mu) and slope (Lambda) of the gamma distribution of raindrops to reduce the number of parameters required to measure rainfall by remote sensing methods. However, we find that there are no well-defined mu-Lambda, or associated relations between reflectivity (Z) and rain rate (R) or differential reflectivity for all storms or portions thereof. Rather, there is a general behavior such that A and b ( in the Z = AR(b) relation) and median volume drop diameter D-o all decrease from convective ( C) to stratiform ( S) to transition ( T) rains. The mu-Lambda correlation of the investigators in question appears to be limited to rainfall events which do not include convective rain; it is biased toward S and T rains. They miss the narrow ( large mu), large D-o DSDs of convective rain that are often found to have equilibrium spectra. The dependence of D-o on the strength of the updraft and the findings of others concerning the association with the physics, dynamics, and climate regime strongly suggests that it is necessary to characterize the physical and dynamic nature of the storms in order to select the appropriate remote sensing algorithms. C1 NASA, Goddard Space Flight Ctr, Atmospheres Lab, Greenbelt, MD 20771 USA. Clemson Univ, Dept Phys & Astron, Clemson, SC 29634 USA. RP Atlas, D (reprint author), NASA, Goddard Space Flight Ctr, Atmospheres Lab, Code 613, Greenbelt, MD 20771 USA. EM davnlu@comcast.net NR 26 TC 25 Z9 25 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 AUG 19 PY 2006 VL 33 IS 16 AR L16803 DI 10.1029/2006GL026824 PG 5 WC Geosciences, Multidisciplinary SC Geology GA 076XN UT WOS:000239991800007 ER PT J AU Folkins, I Bernath, P Boone, C Lesins, G Livesey, N Thompson, AM Walker, K Witte, JC AF Folkins, Ian Bernath, P. Boone, C. Lesins, G. Livesey, N. Thompson, A. M. Walker, K. Witte, J. C. TI Seasonal cycles of O-3, CO, and convective outflow at the tropical tropopause SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID UPPER TROPOSPHERE; OZONE CLIMATOLOGY; DEEP CONVECTION; WATER-VAPOR; ART.; OZONESONDES; SPECTROMETER; VARIABILITY; BALANCE AB Measurements from the SHADOZ ozonesonde network and Aura MLS are used to show that there are seasonal cycles in ozone (O-3) and carbon monoxide (CO) at the tropical tropopause ( similar to 17 km). A simple model, driven by cloud free radiative mass fluxes, is used to investigate the origin of these seasonal cycles. The seasonal cycle in O-3 is due to seasonal changes in upwelling and high altitude convective outflow. The seasonal cycle in CO at 100 hPa is influenced by both seasonal changes in dynamics and seasonal changes in CO at lower altitudes. The age of air at 17 km varies from 40 days during NH winter to 70 days during NH summer. The seasonal cycle in clear sky radiative heating at the tropical tropopause is mainly due to seasonal cycles in O-3 and temperature. The seasonal cycle in O-3 can be expected to amplify the seasonal cycle in cold point temperature. C1 Dalhousie Univ, Dept Phys & Atmospher Sci, Halifax, NS B3H 3J5, Canada. Univ Waterloo, Dept Chem, Waterloo, ON N2L 3G1, Canada. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. Penn State Univ, Dept Meteorol, University Pk, PA 16802 USA. NASA, Goddard Space Flight Ctr, Sci Syst & Applicat Inc, Greenbelt, MD 20770 USA. RP Folkins, I (reprint author), Dalhousie Univ, Dept Phys & Atmospher Sci, Halifax, NS B3H 3J5, Canada. EM ian.folkins@dal.ca RI Bernath, Peter/B-6567-2012; Thompson, Anne /C-3649-2014 OI Bernath, Peter/0000-0002-1255-396X; Thompson, Anne /0000-0002-7829-0920 NR 21 TC 48 Z9 49 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 AUG 19 PY 2006 VL 33 IS 16 AR L16802 DI 10.1029/2006GL026602 PG 5 WC Geosciences, Multidisciplinary SC Geology GA 076XN UT WOS:000239991800005 ER PT J AU Anderson, FS Smrekar, SE AF Anderson, F. Scott Smrekar, Suzanne E. TI Global mapping of crustal and lithospheric thickness on Venus SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Article ID OF-SIGHT ACCELERATIONS; MANTLE FLOW TECTONICS; ELASTIC THICKNESS; ISOSTATIC COMPENSATION; INTERNAL STRUCTURE; TOPOGRAPHIC RISES; ORDER MODEL; HOT-SPOT; GRAVITY; DEFORMATION AB [1] We have produced a high-resolution global admittance map of Venus using a spatiospectral localization technique, calculating 64,800 admittance spectra evenly spaced in latitude and longitude. We grouped the admittance spectra into 35 classes that we inverted for elastic, crustal, and lithospheric thickness using bottom-loading, top-loading, and short-wavelength top-loading models with long-wavelength bottom-loading ("hot spot'') models. Our best fit models identify 17 classes consistent with top loading (40% of the surface), 7 with bottom loading (39%), and 4 with a long-wavelength bottom-loading model (15%). The remaining seven classes (6% of the surface) generally had large-amplitude top-loading signatures that could not be fit with our models. For the classes that were successfully modeled the estimated range of crustal ( 0 - 90 km) and elastic thickness ( 0 - 100 km) is larger than results for most previous studies, primarily because of the incorporation of bottom loading. Nearly half of the planet has elastic thickness < 20 km, which we cannot distinguish from isostasy, suggesting that these regions are tectonically inactive. A key finding is that the lithospheric properties typically vary over scales of 1000 km or less except in some plains and crustal plateau regions. Both the scale and range of crustal and elastic thickness variations indicate that Venus remains an active planet and that geologic processes may be more complex than previously recognized. In many regions the correlation with surface geology is not obvious, and this suggests that deformation of the lower lithosphere and crust may occur with little surface manifestation. C1 Univ Hawaii Manoa, Hawaii Inst Geophys & Planetol, Honolulu, HI 96822 USA. CALTECH, Jet Prop Lab, Pasadena, CA USA. RP Anderson, FS (reprint author), Univ Hawaii Manoa, Hawaii Inst Geophys & Planetol, 1680 East West Rd,POST 526B, Honolulu, HI 96822 USA. EM anderson@higp.hawaii.edu NR 77 TC 35 Z9 36 U1 0 U2 6 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0148-0227 J9 J GEOPHYS RES-PLANET JI J. Geophys. Res.-Planets PD AUG 19 PY 2006 VL 111 IS E8 AR E08006 DI 10.1029/2004JE002395 PG 20 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 076YC UT WOS:000239993500001 ER PT J AU Kwok, R AF Kwok, Ron TI Exchange of sea ice between the Arctic Ocean and the Canadian Arctic Archipelago SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID VARIABILITY; STRAIT; SUMMER; FLUX AB First estimates of sea ice exchange between the Arctic Ocean and the Canadian Arctic Archipelago (CAA) are obtained using six years ( 1997 - 2002) of RADARSAT ice motion. Over the period, the mean annual flux of sea ice area from the Amundsen Gulf (AG), M'Clure Strait ( MS), and Queen Elizabeth Islands (QEI) are - 85 +/- 26 x 10(3), - 20 +/- 24 x 10(3), and 8 +/- 6 x 10(3) km(2). Positive/negative sign indicates Arctic outflow/ inflow. Overall, net sea ice area is exported from the CAA; rough estimates suggest a mean annual volume flux of similar to 10(2) km(3) into the Canada Basin. Ice types are largely seasonal near the AG flux gate, mixed seasonal and multiyear at the MS gate, and primarily multiyear at the QEI gates. Sea ice at the QEI flux gates remains land fast for most of the year. Cross-strait gradient in sea level pressure explains more than 50% of the variance in the area flux at these passages. The role of ice exchange during the anomalous decrease in multiyear ice coverage in the Sverdrup Basin during September 1998 is examined. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Kwok, R (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM ron.kwow@jpl.nasa.gov RI Kwok, Ron/A-9762-2008 OI Kwok, Ron/0000-0003-4051-5896 NR 15 TC 42 Z9 43 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 AUG 18 PY 2006 VL 33 IS 16 AR L16501 DI 10.1029/2006GL027094 PG 5 WC Geosciences, Multidisciplinary SC Geology GA 076XM UT WOS:000239991700006 ER PT J AU Leblanc, T Tripathi, OP McDermid, IS Froidevaux, L Livesey, NJ Read, WG Waters, JW AF Leblanc, Thierry Tripathi, Om Prakash McDermid, I. Stuart Froidevaux, Lucien Livesey, N. J. Read, W. G. Waters, J. W. TI Simultaneous lidar and EOS MLS measurements, and modeling, of a rare polar ozone filament event over Mauna Loa Observatory, Hawaii SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID AURA SATELLITE; TRANSPORT; STRATOSPHERE; CHEMISTRY; VORTEX; SYSTEM; WINTER AB In mid-March 2005, a rare lower stratospheric polar vortex filamentation event was observed simultaneously by the JPL lidar at Mauna Loa Observatory, Hawaii, and by the EOS MLS instrument onboard the Aura satellite. The event coincided with the beginning of the spring 2005 final warming. On 16 March, the filament was observed by lidar around 0600 UT between 415 K and 455 K, and by MLS six hours earlier. It was seen on both the lidar and MLS profiles as a layer of enhanced ozone, peaking at 1.7 ppmv in a region where the climatological values are usually around or below 1 ppmv. Ozone profiles measured by lidar and MLS were compared to profiles from the Chemical Transport Model MIMOSA-CHIM. The agreement between lidar, MLS, and the model is excellent considering the difference in the sampling techniques. MLS was also able to identify the filament at another location north of Hawaii. C1 CALTECH, Jet Prop Lab, Table Mt Facil, Wrightwood, CA 92397 USA. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Leblanc, T (reprint author), CALTECH, Jet Prop Lab, Table Mt Facil, 24490 Table Mt Rd, Wrightwood, CA 92397 USA. EM leblanc@tmf.jpl.nasa.gov NR 14 TC 9 Z9 9 U1 0 U2 0 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 EI 1944-8007 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD AUG 18 PY 2006 VL 33 IS 16 AR L16801 DI 10.1029/2006GL026257, PG 4 WC Geosciences, Multidisciplinary SC Geology GA 076XM UT WOS:000239991700001 ER PT J AU Chiu, JC Marshak, A Knyazikhin, Y Wiscombe, WJ Barker, HW Barnard, JC Luo, Y AF Chiu, J. Christine Marshak, Alexander Knyazikhin, Yuri Wiscombe, Warren J. Barker, Howard W. Barnard, James C. Luo, Yi TI Remote sensing of cloud properties using ground-based measurements of zenith radiance SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID OPTICAL DEPTH; VEGETATION; RETRIEVAL; SCATTERING; RADIOMETER; THICKNESS; ALGORITHM; ALBEDO AB [1] We have conducted the first extensive field test of two new methods to retrieve optical properties for overhead clouds that range from patchy to overcast. The methods use measurements of zenith radiance at 673 and 870 nm wavelengths and require the presence of green vegetation in the surrounding area. The test was conducted at the Atmospheric Radiation Measurement Program Oklahoma site during September - November 2004. These methods work because at 673 nm ( red) and 870 nm ( near infrared (NIR)), clouds have nearly identical optical properties, while vegetated surfaces reflect quite differently. The first method, dubbed REDvsNIR, retrieves not only cloud optical depth tau but also radiative cloud fraction. Because of the 1-s time resolution of our radiance measurements, we are able for the first time to capture changes in cloud optical properties at the natural timescale of cloud evolution. We compared values of tau retrieved by REDvsNIR to those retrieved from downward shortwave fluxes and from microwave brightness temperatures. The flux method generally underestimates tau relative to the REDvsNIR method. Even for overcast but inhomogeneous clouds, differences between REDvsNIR and the flux method can be as large as 50%. In addition, REDvsNIR agreed to better than 15% with the microwave method for both overcast and broken clouds. The second method, dubbed COUPLED, retrieves tau by combining zenith radiances with fluxes. While extra information from fluxes was expected to improve retrievals, this is not always the case. In general, however, the COUPLED and REDvsNIR methods retrieve tau to within 15% of each other. C1 Univ Maryland Baltimore Cty, Joint Ctr Earth Syst Technol, Baltimore, MD 21250 USA. NASA, Climate & Radiat Branch, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Boston Univ, Dept Geog, Boston, MA 02215 USA. Meteorol Serv Canada, Cloud Phys Res Div, Downsview, ON M3H 5T4, Canada. Pacific NW Natl Lab, Richland, WA 99352 USA. Nat Resources Canada, Canada Ctr Remote Sensing, Ottawa, ON K1A 0Y7, Canada. RP Chiu, JC (reprint author), Univ Maryland Baltimore Cty, Joint Ctr Earth Syst Technol, 1000 Hilltop Circle, Baltimore, MD 21250 USA. EM cchiu@climate.gsfc.nasa.gov RI Wiscombe, Warren/D-4665-2012; Chiu, Christine/E-5649-2013; Marshak, Alexander/D-5671-2012 OI Wiscombe, Warren/0000-0001-6844-9849; Chiu, Christine/0000-0002-8951-6913; NR 23 TC 23 Z9 23 U1 0 U2 2 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD AUG 18 PY 2006 VL 111 IS D16 AR D16201 DI 10.1029/2005JD006843 PG 12 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 076XS UT WOS:000239992400004 ER PT J AU Tuthill, P Monnier, J Tanner, A Figer, D Ghez, A Danchi, W AF Tuthill, Peter Monnier, John Tanner, Angelle Figer, Donald Ghez, Andrea Danchi, William TI Pinwheels in the quintuplet cluster SO SCIENCE LA English DT Article ID GALACTIC-CENTER; NEBULA; STARS C1 Univ Sydney, Dept Phys, Sydney, NSW 2006, Australia. Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. Rochester Inst Technol, COS Ctr Imaging Sci, Rochester, NY 14623 USA. Univ Calif Los Angeles, Los Angeles, CA 90095 USA. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Tuthill, P (reprint author), Univ Sydney, Dept Phys, Sydney, NSW 2006, Australia. EM p.tuthill@physics.usyd.edu.au NR 10 TC 42 Z9 42 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 AUG 18 PY 2006 VL 313 IS 5789 BP 935 EP 935 DI 10.1126/science.1128731 PG 1 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 074MR UT WOS:000239817000033 PM 16917053 ER PT J AU Searls, ML Banerdt, WB Phillips, RJ AF Searls, Mindi L. Banerdt, W. Bruce Phillips, Roger J. TI Utopia and Hellas basins, Mars: Twins separated at birth SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Article ID ORBITER LASER ALTIMETER; INTERNAL STRUCTURE; GLOBAL SURVEYOR; CRUSTAL EVOLUTION; NORTHERN LOWLANDS; THERMAL EVOLUTION; GRAVITY-FIELD; MARTIAN CRUST; TOPOGRAPHY; THICKNESS AB [1] Using topography and gravity data as constraints, we formulate spherical harmonic thin elastic-shell models to determine the subsurface structure of the Hellas and Utopia basins. For Hellas, we show that our model is consistent with the elastic thickness results of McGovern et al. ( 2002, 2004). The thin elastic lithosphere at the time of formation implies that Hellas is close to isostatic. Since Utopia formed earlier, we argue that an isostatic assumption is justified for the Utopia basin before it was filled. From this supposition, we derive a system of equations that allows us to solve for the amount of fill, the prefill topography, and the amount of flexure due to the fill within the Utopia basin. An analysis of the parameter space shows that the fill density and the amount of fill is strongly dependent on the elastic thickness at the time of infilling. A thinner elastic lithosphere favors a denser fill, while a thicker lithosphere will allow for less dense material. Likewise, larger crustal thickness values lead to smaller fill density values. The presence of quasi-circular depressions, interpreted as impact craters, within the Utopia basin indicates that the majority of the material within Utopia was deposited prior to 4.04 - 4.11 Ga. The early timing for the deposition combined with the heat imparted by the basin forming event argues for a thinner lithosphere which could, in turn, suggest fill densities that are more consistent with a volcanic load than with pure sediment or ice-rich material. These results are supported using an alternative method of determining the amount of fill and flexure within Utopia. This model assumes that Hellas and Utopia were initially identical and that the only difference in their subsequent evolution was the addition of material in the Utopia basin. The volume of material needed to fill Utopia is immense ( on the order of 50 million km 3 or more). The high density obtained for the fill requires that it contain a large igneous component, the source of which is problematic. Relaxing the isostatic assumption to a reasonable degree perturbs the density bound only slightly. C1 Washington Univ, Dept Earth & Planetary Sci, St Louis, MO 63130 USA. Washington Univ, McDonnell Ctr Space Sci, St Louis, MO 63130 USA. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Searls, ML (reprint author), Washington Univ, Dept Earth & Planetary Sci, Campus Box 1169,1 Brookings Dr, St Louis, MO 63130 USA. EM mlsearls@artsci.wustl.edu NR 46 TC 10 Z9 10 U1 0 U2 3 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0148-0227 J9 J GEOPHYS RES-PLANET JI J. Geophys. Res.-Planets PD AUG 17 PY 2006 VL 111 IS E8 AR E08005 DI 10.1029/2005JE002666 PG 13 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 076YB UT WOS:000239993400002 ER PT J AU Michaels, TI Colaprete, A Rafkin, SCR AF Michaels, T. I. Colaprete, A. Rafkin, S. C. R. TI Significant vertical water transport by mountain-induced circulations on Mars SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID ICE CLOUDS; MARTIAN ATMOSPHERE; SEASONAL BEHAVIOR; MODEL; APHELION AB Using a 3-D, non-hydrostatic mesoscale Mars atmospheric model with detailed aerosol/cloud microphysics, we show that the formation of discrete afternoon clouds over the Olympus Mons volcano is due to the symbiosis of upslope thermal flow and a lee mountain wave circulation, and that these clouds exhibit complex particle distributions. Furthermore, we illustrate that this and other mountain-induced circulations transport large quantities of dust, water vapor, and water ice aerosol from lower altitudes into the free atmosphere general circulation. Therefore, these circulations are an important part of Mars' net Hadley circulation and climatic forcing. C1 SW Res Inst, Dept Space Studies, Boulder, CO 80302 USA. NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Michaels, TI (reprint author), SW Res Inst, Dept Space Studies, 1050 Walnut St,Suite 400, Boulder, CO 80302 USA. EM tmichael@boulder.swri.edu; anthony.colaprete-1@nasa.gov NR 24 TC 43 Z9 43 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 AUG 16 PY 2006 VL 33 IS 16 AR L16201 DI 10.1029/2006GL026562 PG 5 WC Geosciences, Multidisciplinary SC Geology GA 076XK UT WOS:000239991500003 ER PT J AU Kwok, R AF Kwok, R. TI Contrasts in sea ice deformation and production in the Arctic seasonal and perennial ice zones SO JOURNAL OF GEOPHYSICAL RESEARCH-OCEANS LA English DT Article ID SYNTHETIC-APERTURE RADAR; GEOPHYSICAL PROCESSOR SYSTEM; HIGH-RESOLUTION RADIOMETER; VOLUME PRODUCTION; MOTION; THIN; THICKNESS; SHEBA; OCEAN; PARAMETERIZATIONS AB [ 1] Four years ( 1997 - 2000) of RADARSAT Geophysical Processor System (RGPS) data are used to contrast the sea ice deformation and production regionally, and in the seasonal (SIZ) and perennial (PIZ) ice zones. Ice production is of seasonal ice in openings during the winter. Three-day estimates of these quantities are provided within Lagrangian elements initially 10 km on a side. A distinct seasonal cycle is seen in both zones with these estimates highest in the late fall and with seasonal minimums in the midwinter. Regional divergence over the winter could be up to 30%. Spatially, the highest deformation is seen in the SIZ north of coastal Alaska. Both ice deformation and production are higher in the SIZ: deformation-related ice production in the SIZ ( similar to 0.5 m) is 1.5 - 2.3 times that of the PIZ ( similar to 0.3 m): this is connected to ice strength and thickness. Atmospheric forcing and boundary layer structure contribute to only the seasonal and interannual variability. Seasonal ice growth in ice fractures accounts for similar to 25 - 40% of the total ice production of the Arctic Ocean. Uncertainties in these estimates are discussed. By itself, this deformation-ice production relationship could be considered a negative feedback when thickness is perturbed. However, the overall effect on ice production in the face of increasing seasonal and thinner/weaker ice coverage could be modified by local destabilization of the water column promoting overturning of warmer water due to increased brine rejection; and the upwelling of the pynocline associated with increased occurrence of large shear motion in sea ice. Divergence is shown to be negligibly correlated to cyclonic motion in summer and winter in both ice zones. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Kwok, R (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM ron.kwok@jpl.nasa.gov RI Kwok, Ron/A-9762-2008 OI Kwok, Ron/0000-0003-4051-5896 NR 37 TC 28 Z9 28 U1 1 U2 4 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9275 EI 2169-9291 J9 J GEOPHYS RES-OCEANS JI J. Geophys. Res.-Oceans PD AUG 16 PY 2006 VL 111 IS C11 AR C11S22 DI 10.1029/2005JC003246 PG 14 WC Oceanography SC Oceanography GA 076YA UT WOS:000239993300001 ER PT J AU Higashibata, A Szewczyk, NJ Conley, CA Imamizo-Sato, M Higashitani, A Ishioka, N AF Higashibata, Akira Szewczyk, Nathaniel J. Conley, Catharine A. Imamizo-Sato, Mari Higashitani, Atsushi Ishioka, Noriaki TI Decreased expression of myogenic transcription factors and myosin heavy chains in Caenorhabditis elegans muscles developed during spaceflight SO JOURNAL OF EXPERIMENTAL BIOLOGY LA English DT Article DE spaceflight; muscle remodeling; Caenorhabditis elegans; myosin heavy chain; development ID PROMOTES PROTEIN-DEGRADATION; SKELETAL-MUSCLE; GENE-EXPRESSION; CONTRACTILE PROPERTIES; PHARYNGEAL MUSCLE; SOLEUS MUSCLE; MICROGRAVITY; PARAMYOSIN; ISOFORMS; ATROPHY AB The molecular mechanisms underlying muscle atrophy during spaceflight are not well understood. We have analyzed the effects of a 10-day spaceflight on Caenorhabditis elegans muscle development. DNA microarray, real-time quantitative PCR, and quantitative western blot analyses revealed that the amount of MHC in both body-wall and pharyngeal muscle decrease in response to spaceflight. Decreased transcription of the body-wall myogenic transcription factor HLH-1 ( CeMyoD) and of the three pharyngeal myogenic transcription factors, PEB-1, CEH-22 and PHA-4 were also observed. Upon return to Earth animals displayed reduced rates of movement, indicating a functional defect. These results demonstrate that C. elegans muscle development is altered in response to spaceflight. This altered development occurs at the level of gene transcription and was observed in the presence of innervation, not simply in isolated cells. This important finding coupled with past observations of decreased levels of the same myogenic transcription factions in vertebrates after spaceflight raises the possibility that altered muscle development is a contributing factor to spaceflight-induced muscle atrophy in vertebrates. C1 Japan Aerosp Explorat Agcy, Tsukuba, Ibaraki 3058505, Japan. NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. Adv Engn Serv Co Ltd, Tsukuba, Ibaraki 3050032, Japan. Tohoku Univ, Grad Sch Life Sci, Sendai, Miyagi 9808577, Japan. RP Higashibata, A (reprint author), Univ Pittsburgh, Dept Biol Sci, A234 Langley Hall,4249 5th Ave, Pittsburgh, PA 15260 USA. EM higashibata.akira@jaxa.jp RI Higashitani, Atsushi/G-7086-2015; OI Higashitani, Atsushi/0000-0001-6920-0594; Szewczyk, Nathaniel/0000-0003-4425-9746 NR 55 TC 27 Z9 42 U1 1 U2 8 PU COMPANY OF BIOLOGISTS LTD PI CAMBRIDGE PA BIDDER BUILDING CAMBRIDGE COMMERCIAL PARK COWLEY RD, CAMBRIDGE CB4 4DL, CAMBS, ENGLAND SN 0022-0949 J9 J EXP BIOL JI J. Exp. Biol. PD AUG 15 PY 2006 VL 209 IS 16 BP 3209 EP 3218 DI 10.1242/jeb.02365 PG 10 WC Biology SC Life Sciences & Biomedicine - Other Topics GA 071ZB UT WOS:000239641300020 PM 16888068 ER PT J AU Podesta, JJ AF Podesta, J. J. TI Radial decay law for large-scale velocity and magnetic field fluctuations in the solar wind SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article ID MAGNETOHYDRODYNAMIC TURBULENCE; WAVES; HELIOSPHERE; EVOLUTION; DISTANCE; 1-AU AB [ 1] Solar wind data from Helios 1 and 2 and from Voyager 1 and 2 are used to show that between 0.3 and 20 AU in the ecliptic plane, the total energy per unit mass contained in the velocity and magnetic field fluctuations decays approximately as a power law of the form R-alpha, where R is the heliocentric distance in astronomical units ( AU) and - 0.64 <= alpha <= -0.41. It is also shown that to the first order of approximation, this quantity is independent of the effects of solar cycle variations. An analysis of OMNI data at 1 AU from 1969 through 2002 shows that the Alfven ratio, the ratio of kinetic energy to magnetic energy in the fluctuations, exhibits large solar cycle variations rising from 1 or 2 at solar maximum to 8 or 9 either near solar minimum or a couple of years before minimum. This is due to the fact that the kinetic and magnetic energy in the fluctuations both undergo solar cycle variations, with the kinetic energy increasing to a maximum around solar minimum and the magnetic energy decreasing to a minimum around solar minimum. It is found that these effects appear to offset each other so that the sum of the kinetic plus magnetic energies does not exhibit noticeable solar cycle variations. C1 NASA, Lab Solar & Space Phys, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Podesta, JJ (reprint author), NASA, Lab Solar & Space Phys, Goddard Space Flight Ctr, Code 612-2, Greenbelt, MD 20771 USA. EM jpodesta@solar.stanford.edu NR 19 TC 0 Z9 0 U1 0 U2 0 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0148-0227 J9 J GEOPHYS RES-SPACE JI J. Geophys. Res-Space Phys. PD AUG 15 PY 2006 VL 111 IS A8 AR A08103 DI 10.1029/2005JA011528 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 076YH UT WOS:000239994000001 ER PT J AU Gamon, JA Rahman, AF Dungan, JL Schildhauer, M Huemmrich, KF AF Gamon, J. A. Rahman, A. F. Dungan, J. L. Schildhauer, M. Huemmrich, K. F. TI Spectral Network (SpecNet) - What is it and why do we need it? SO REMOTE SENSING OF ENVIRONMENT LA English DT Article DE SpecNet (Spectral Network); optical remote sensing; surface-atmosphere flux; scaling; satellite validation; FLUXNET ID GROSS PRIMARY PRODUCTION; LIGHT-USE EFFICIENCY; ATMOSPHERIC CO2; BOREAL FOREST; EARTH-SCIENCE; LEAF; PHOTOSYNTHESIS; MODEL; MODIS; VALIDATION AB Effective integration of optical remote sensing with flux measurements across multiple scales is essential for understanding global patterns of surface-atmosphere fluxes of carbon and water vapor. SpecNet (Spectral Network) is an international network of cooperating investigators and sites linking optical measurements with flux sampling for the purpose of improving our understanding of the controls on these fluxes. An additional goal is to characterize disturbance impacts on surface-atmosphere fluxes. To reach these goals, key SpecNet objectives include the exploration of scaling issues, development of novel sampling tools, standardization and intercomparison of sampling methods, development of models and statistical methods that relate optical sampling to fluxes, exploration of component fluxes, validation of satellite products, and development of an informatics approach that integrates disparate data sources across scales. Examples of these themes are summarized in this review. (c) 2006 Elsevier Inc. All rights reserved. C1 Calif State Univ Los Angeles, Dept Biol Sci, Los Angeles, CA 90032 USA. Texas Tech Univ, MS2125, Lubbock, TX 79409 USA. NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. Natl Ctr Ecol Anal & Synth, Santa Barbara, CA 93101 USA. Univ Maryland Baltimore Cty, NASA, GSFC, Joint Ctr Earth Syst Technol, Greenbelt, MD 20771 USA. RP Gamon, JA (reprint author), Calif State Univ Los Angeles, Dept Biol Sci, 5151 State Unite Dr, Los Angeles, CA 90032 USA. EM jgamon@gmail.com RI Gamon, John/A-2641-2014; Dungan, Jennifer/G-9921-2016; OI Gamon, John/0000-0002-8269-7723; Dungan, Jennifer/0000-0002-4863-1616; Schildhauer, Mark/0000-0003-0632-7576 NR 46 TC 78 Z9 81 U1 1 U2 30 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 AUG 15 PY 2006 VL 103 IS 3 BP 227 EP 235 DI 10.1016/j.rse.2006.04.003 PG 9 WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic Technology SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science & Photographic Technology GA 075JS UT WOS:000239881600001 ER PT J AU Ju, S Lee, K Janes, DB Dwivedi, RC Baffour-Awuah, H Wilkins, R Yoon, MH Facchetti, A Mark, TJ AF Ju, Sanghyun Lee, Kangho Janes, David B. Dwivedi, Ramesh C. Baffour-Awuah, Habibah Wilkins, R. Yoon, Myung-Han Facchetti, Antonio Mark, Tobin J. TI Proton radiation hardness of single-nanowire transistors using robust organic gate nanodielectrics SO APPLIED PHYSICS LETTERS LA English DT Article ID THIN-FILM TRANSISTORS; DEVICES AB In this contribution, the radiation tolerance of single ZnO nanowire field-effect transistors (NW-FETs) fabricated with a self-assembled superlattice (SAS) gate insulator is investigated and compared with that of ZnO NW-FETs fabricated with a 60 nm SiO2 gate insulator. A total-radiation dose study was performed using 10 MeV protons at doses of 5.71 and 285 krad(Si). The threshold voltage (V-th) of the SAS-based ZnO NW-FETs is not shifted significantly following irradiation at these doses. In contrast, V-th parameters of the SiO2-based ZnO NW-FETs display average shifts of similar to-4.0 and similar to-10.9 V for 5.71 and 285 krad(Si) H+ irradiation, respectively. In addition, little change is observed in the subthreshold characteristics (off current, subthreshold slope) of the SAS-based ZnO NW-FETs following H+ irradiation. These results strongly argue that the bulk oxide trap density and interface trap density formed within the SAS and/or at the SAS-ZnO NW interface during H+ irradiation are significantly lower than those for the corresponding SiO2 gate dielectrics. The radiation-robust SAS-based ZnO NW-FETs are thus promising candidates for future space-based applications in electronics and flexible displays. (c) 2006 American Institute of Physics. C1 Purdue Univ, Sch Elect & Comp Engn, Inst Nanoelect & Comp, W Lafayette, IN 47907 USA. Purdue Univ, Birck Nanotechnol Ctr, W Lafayette, IN 47907 USA. Prairie View A&M Univ, NASA, CARR, Prairie View, TX USA. Prairie View A&M Univ, Dept Elect Engn, Prairie View, TX USA. Northwestern Univ, Dept Chem, Evanston, IL 60208 USA. Northwestern Univ, Mat Res Ctr, Evanston, IL 60208 USA. Northwestern Univ, Inst Nanoelect & Comp, Evanston, IL 60208 USA. RP Janes, DB (reprint author), Purdue Univ, Sch Elect & Comp Engn, Inst Nanoelect & Comp, W Lafayette, IN 47907 USA. EM janes@ecn.purdue.edu; rtwilkins@pvamu.edu; t-marks@northwestern.edu NR 14 TC 20 Z9 20 U1 0 U2 10 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 AUG 14 PY 2006 VL 89 IS 7 AR 073510 DI 10.1063/1.2336744 PG 3 WC Physics, Applied SC Physics GA 074WL UT WOS:000239842400092 ER PT J AU Eckermann, SD Wu, DL AF Eckermann, S. D. Wu, D. L. TI Imaging gravity waves in lower stratospheric AMSU-A radiances, Part 1: Simple forward model SO ATMOSPHERIC CHEMISTRY AND PHYSICS LA English DT Article ID ATMOSPHERIC-TEMPERATURE; MICROWAVE SPECTROMETER; SATELLITE-OBSERVATIONS; SOLVE/THESEO 2000; MORPHOLOGY; VARIANCE; LIMB; INSTRUMENTS; CALIBRATION; VALIDATION AB Using a simplified model of in-orbit radiance acquisition by the Advanced Microwave Sounding Unit (AMSU-A), we derive three-dimensional temperature weighting functions for Channel 9 measurements (peaking at similar to 60-90 hPa) at all 30 cross-track beam positions and use them to investigate the sensitivity of these radiances to gravity waves. The vertical widths of the weighting functions limit detection to waves with vertical wavelengths of greater than or similar to 10 km, with slightly better vertical wavelength sensitivity at the outermost scan angles due to the limb effect. Fourier Transforms of two-dimensional cross-track weighting functions reveal optimal sensitivity to cross-track wavelengths at the near-nadir scan angles, where horizontal measurement footprints are smallest. This sensitivity is greater for the AMSU-A on the Aqua satellite than for the identical instruments on the NOAA meteorological satellites, due to a lower orbit altitude and thus smaller horizontal footprints from antenna spreading. Small cross-track asymmetries in the radiance response to gravity waves are found that peak at the mid-range scan angles, with more symmetric responses at near-nadir and far off-nadir scan angles. Three-dimensional simulations show gravity wave oscillations imaged in horizontal AMSU-A radiance maps swept out by the scan pattern and satellite motion. A distorting curvature is added to imaged wave phase lines due to vertical variations in weighting function peaks with cross-track scan angle. This wave distortion is analogous to the well-known "limb darkening" and "limb brightening" of microwave radiances acquired from purely vertical background temperature profiles by cross-track scanners. Waves propagating along track are more visible in these images at the outermost scan angles than those propagating cross track, due to oversampling and narrower widths of the horizontal measurement footprints in the along track direction. Based on nominal noise floors and representative lower stratospheric wave temperature amplitudes, our modeling indicates that Channel 9 AMSU-A radiances can resolve and horizontally image gravity waves with horizontal wavelengths of greater than or similar to 150 km and vertical wavelengths of greater than or similar to 10 km. C1 USN, Res Lab, EO Hulburt Ctr Space Res, Washington, DC 20375 USA. CALTECH, Jet Prop Lab, Pasadena, CA USA. RP Eckermann, SD (reprint author), USN, Res Lab, EO Hulburt Ctr Space Res, Washington, DC 20375 USA. EM stephen.eckermann@nrl.navy.mil RI Wu, Dong/D-5375-2012 NR 35 TC 9 Z9 9 U1 0 U2 2 PU COPERNICUS GESELLSCHAFT MBH PI GOTTINGEN PA BAHNHOFSALLEE 1E, GOTTINGEN, 37081, GERMANY SN 1680-7316 EI 1680-7324 J9 ATMOS CHEM PHYS JI Atmos. Chem. Phys. PD AUG 14 PY 2006 VL 6 BP 3325 EP 3341 PG 17 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 074RI UT WOS:000239829100001 ER PT J AU Eckermann, SD Wu, DL Doyle, JD Burris, JF Mcgee, TJ Hostetler, CA Coy, L Lawrence, BN Stephens, A McCormack, JP Hogan, TF AF Eckermann, S. D. Wu, D. L. Doyle, J. D. Burris, J. F. McGee, T. J. Hostetler, C. A. Coy, L. Lawrence, B. N. Stephens, A. McCormack, J. P. Hogan, T. F. TI Imaging gravity waves in lower stratospheric AMSU-A radiances, Part 2: Validation case study SO ATMOSPHERIC CHEMISTRY AND PHYSICS LA English DT Article ID ECMWF FORECAST MODEL; MOUNTAIN WAVES; TEMPERATURE-MEASUREMENTS; SOLVE/THESEO 2000; UNIFIED MODEL; SIMULATIONS; CAMPAIGN; CLOUDS; OZONE; LIMB AB Two-dimensional radiance maps from Channel 9 (similar to 60-90 hPa) of the Advanced Microwave Sounding Unit (AMSU-A), acquired over southern Scandinavia on 14 January 2003, show plane-wave-like oscillations with a wavelength lambda(h) of similar to 400-500 km and peak brightness temperature amplitudes of up to 0.9 K. The wave-like pattern is observed in AMSU-A radiances from 8 overpasses of this region by 4 different satellites, revealing a growth in the disturbance amplitude from 00:00 UTC to 12:00 UTC and a change in its horizontal structure between 12:00 UTC and 20:00 UTC. Forecast and hindcast runs for 14 January 2003 using high-resolution global and regional numerical weather prediction (NWP) models generate a lower stratospheric mountain wave over southern Scandinavia with peak 90 hPa temperature amplitudes of similar to 5-7K at 12:00 UTC and a similar horizontal wavelength, packet width, phase structure and time evolution to the disturbance observed in AMSU-A radiances. The wave's vertical wavelength is similar to 12 km. These NWP fields are validated against radiosonde wind and temperature profiles and airborne lidar profiles of temperature and aerosol backscatter ratios acquired from the NASA DC-8 during the second SAGE III Ozone Loss and Validation Experiment (SOLVE II). Both the amplitude and phase of the stratospheric mountain wave in the various NWP fields agree well with localized perturbation features in these suborbital measurements. In particular, we show that this wave formed the type II polar stratospheric clouds measured by the DC-8 lidar. To compare directly with the AMSU-A data, we convert these validated NWP temperature fields into swath-scanned brightness temperatures using three-dimensional Channel 9 weighting functions and the actual AMSU-A scan patterns from each of the 8 overpasses of this region. These NWP-based brightness temperatures contain two-dimensional oscillations due to this resolved stratospheric mountain wave that have an amplitude, wavelength, horizontal structure and time evolution that closely match those observed in the AMSU-A data. These comparisons not only verify gravity wave detection and horizontal imaging capabilities for AMSU-A Channel 9, but provide an absolute validation of the anticipated radiance signals for a given three-dimensional gravity wave, based on the modeling of Eckermann and Wu (2006). C1 USN, Res Lab, EO Hulburt Ctr Space Res, Washington, DC 20375 USA. CALTECH, Jet Prop Lab, Pasadena, CA USA. USN, Marine Meteorol Div, Res Lab, Monterey, CA USA. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. NASA, Langley Res Ctr, Hampton, VA 23665 USA. Rutherford Appleton Lab, British Atmospher Data Ctr, Didcot, Oxon, England. RP Eckermann, SD (reprint author), USN, Res Lab, EO Hulburt Ctr Space Res, Washington, DC 20375 USA. EM eckermann@nrl.navy.mil RI McGee, Thomas/G-4951-2013; Wu, Dong/D-5375-2012; OI McCormack, John/0000-0002-3674-0508; Lawrence, Bryan/0000-0001-9262-7860 NR 54 TC 28 Z9 28 U1 1 U2 8 PU COPERNICUS GESELLSCHAFT MBH PI GOTTINGEN PA BAHNHOFSALLEE 1E, GOTTINGEN, 37081, GERMANY SN 1680-7316 J9 ATMOS CHEM PHYS JI Atmos. Chem. Phys. PD AUG 14 PY 2006 VL 6 BP 3343 EP 3362 PG 20 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 074RI UT WOS:000239829100002 ER PT J AU Hong, Y Hsu, KL Moradkhani, H Sorooshian, S AF Hong, Yang Hsu, Kuo-lin Moradkhani, Hamid Sorooshian, Soroosh TI Uncertainty quantification of satellite precipitation estimation and Monte Carlo assessment of the error propagation into hydrologic response SO WATER RESOURCES RESEARCH LA English DT Article ID ARTIFICIAL NEURAL-NETWORK; GLOBAL PRECIPITATION; RAINFALL ESTIMATION; PASSIVE-MICROWAVE; FLOOD PREDICTION; RADAR; ALGORITHM; MODEL; SIMULATION; RESOLUTION AB [ 1] The aim of this paper is to foster the development of an end-to-end uncertainty analysis framework that can quantify satellite-based precipitation estimation error characteristics and to assess the influence of the error propagation into hydrological simulation. First, the error associated with the satellite-based precipitation estimates is assumed as a nonlinear function of rainfall space-time integration scale, rain intensity, and sampling frequency. Parameters of this function are determined by using high-resolution satellite-based precipitation estimates and gauge-corrected radar rainfall data over the southwestern United States. Parameter sensitivity analysis at 16 selected 5 degrees x 5 degrees latitude-longitude grids shows about 12 - 16% of variance of each parameter with respect to its mean value. Afterward, the influence of precipitation estimation error on the uncertainty of hydrological response is further examined with Monte Carlo simulation. By this approach, 100 ensemble members of precipitation data are generated, as forcing input to a conceptual rainfall-runoff hydrologic model, and the resulting uncertainty in the streamflow prediction is quantified. Case studies are demonstrated over the Leaf River basin in Mississippi. Compared with conventional procedure, i.e., precipitation estimation error as fixed ratio of rain rates, the proposed framework provides more realistic quantification of precipitation estimation error and offers improved uncertainty assessment of the error propagation into hydrologic simulation. Further study shows that the radar rainfall-generated streamflow sequences are consistently contained by the uncertainty bound of satellite rainfall generated streamflow at the 95% confidence interval. C1 Univ Calif Irvine, Dept Civil & Environm Engn, Ctr Hydrometeorol & Remote Sensing, Irvine, CA 92697 USA. RP Hong, Y (reprint author), NASA, Goddard Space Flight Ctr, Mail Stop 613-1, Greenbelt, MD 20771 USA. EM yanghong@agnes.gsfc.nasa.gov RI Hong, Yang/D-5132-2009; sorooshian, soroosh/B-3753-2008; Moradkhani, Hamid/B-1571-2012 OI Hong, Yang/0000-0001-8720-242X; sorooshian, soroosh/0000-0001-7774-5113; NR 38 TC 80 Z9 81 U1 5 U2 27 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0043-1397 J9 WATER RESOUR RES JI Water Resour. Res. PD AUG 12 PY 2006 VL 42 IS 8 AR W08421 DI 10.1029/2005WR004398 PG 15 WC Environmental Sciences; Limnology; Water Resources SC Environmental Sciences & Ecology; Marine & Freshwater Biology; Water Resources GA 074CJ UT WOS:000239789700001 ER PT J AU Norman, MD Yaxley, GM Bennett, VC Brandon, AD AF Norman, M. D. Yaxley, G. M. Bennett, V. C. Brandon, A. D. TI Magnesium isotopic composition of olivine from the Earth, Mars, Moon, and pallasite parent body SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID SOUTHERN WEST GREENLAND; ITSAQ GNEISS COMPLEX; CARBONATITE METASOMATISM; MANTLE XENOLITHS; INCLUSIONS; AUSTRALIA; ELEMENT; ORIGIN; METEORITES; CHONDRULES AB To investigate the nebular history of material contributing to the terrestrial planets, and search for evidence of a high-temperature origin of the Moon, we measured Mg isotopic compositions of primitive olivines from the Earth, Moon, Mars, and pallasite parent body using laser-ablation multi-collector ICPMS. No temporal variation in the Earth's mantle since at least 3.8 Ga, and only limited variations in the compositions of mantle sources from diverse tectonic settings were found. Earth, Moon, Mars, and differentiated asteroids appear to have formed from a nebular reservoir that was homogeneous with respect to Mg isotopes. This implies either a minor role for evaporation-condensation in the inner solar system, or a limited variation in the proportion of refractory CAI-like material contributing to the terrestrial planets. The Mg isotopic composition of the Moon is identical to the Earth's mantle, placing strong constraints on any volatility-related fractionation that occurred during formation of the Moon. C1 Australian Natl Univ, Res Sch Earth Sci, Canberra, ACT 0200, Australia. Lunar & Planetary Inst, Houston, TX 77058 USA. NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. RP Norman, MD (reprint author), Australian Natl Univ, Res Sch Earth Sci, Canberra, ACT 0200, Australia. EM marc.norman@anu.edu.au RI Yaxley, Greg/A-1167-2008; OI Yaxley, Greg/0000-0003-0445-8812 NR 24 TC 20 Z9 21 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 AUG 11 PY 2006 VL 33 IS 15 AR L15202 DI 10.1029/2006GL026446 PG 5 WC Geosciences, Multidisciplinary SC Geology GA 074BD UT WOS:000239786300002 ER PT J AU Field, CV Schmidt, GA Koch, D Salyk, C AF Field, Christy V. Schmidt, Gavin A. Koch, Dorothy Salyk, Colette TI Modeling production and climate-related impacts on Be-10 concentration in ice cores SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID COSMOGENIC-NUCLIDE PRODUCTION; GENERAL-CIRCULATION MODEL; STRATOSPHERE-TROPOSPHERE EXCHANGE; YOUNGER DRYAS EVENT; BERYLLIUM 10; ANTARCTIC ICE; ATMOSPHERIC TRANSPORT; CENTRAL GREENLAND; SOLAR MODULATION; NORTH-ATLANTIC AB [ 1] The connection between the production of the cosmogenic isotope Be-10 and changes in heliomagnetic activity makes ice core Be-10 an attractive proxy for studying changes in solar output. However, interpreting Be-10 ice core records on centennial timescales is complicated by potential climate-related deposition changes that could obscure the Be-10 production signal. By using the Goddard Institute for Space Studies ModelE general circulation model to selectively vary climate and production functions, we model Be-10 flux at key ice-coring sites. We vary geomagnetic field strength and the solar activity modulation parameter (phi), CO2, sea surface temperatures, and volcanic aerosols to assess impacts on Be-10. Specifically, we find significant latitudinal differences in the response of Be-10 fluxes to changes in the production function. In the climate experiments the Be-10 deposition changes simulated over ice sheets in both hemispheres are comparable to those seen in the production experiments. This altered deposition combined with changes of snow accumulation results in significant climate-related Be-10 concentration variation in both Greenland and Antarctica. Over the Holocene our results suggest that the Be-10 response to climate change should not be neglected when inferring production changes. C1 Columbia Univ, Dept Earth & Environm Sci, New York, NY 10025 USA. Columbia Univ, NASA, Goddard Inst Space Studies, New York, NY 10025 USA. Columbia Univ, Ctr Climate Syst Res, New York, NY 10025 USA. CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. RP Field, CV (reprint author), Columbia Univ, Dept Earth & Environm Sci, 2880 Broadway, New York, NY 10025 USA. EM cfield@giss.nasa.gov RI Schmidt, Gavin/D-4427-2012 OI Schmidt, Gavin/0000-0002-2258-0486 NR 62 TC 92 Z9 92 U1 1 U2 13 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X EI 2169-8996 J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD AUG 11 PY 2006 VL 111 IS D15 AR D15107 DI 10.1029/2005JD006410 PG 13 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 074BK UT WOS:000239787000001 ER PT J AU Davies, RD Dickinson, C Banday, AJ Jaffe, TR Gorski, KM Davis, RJ AF Davies, R. D. Dickinson, C. Banday, A. J. Jaffe, T. R. Gorski, K. M. Davis, R. J. TI A determination of the spectra of Galactic components observed by the Wilkinson Microwave Anisotropy Probe SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE radiation mechanisms : general; cosmic microwave background; cosmology : observations; diffuse radiation; radio continuum : ISM ID INTERSTELLAR-MEDIUM EMISSION; RADIO-CONTINUUM EMISSION; WMAP OBSERVATIONS; POWER-SPECTRUM; SPINNING DUST; HII-REGIONS; 408 MHZ; SKY; GRAINS; RADIATION AB Wilkinson Microwave Anisotropy Probe (WMAP) data when combined with ancillary data on free-free, synchrotron and dust allow an improved understanding of the spectrum of emission from each of these components. Here, we examine the sky variation at intermediate latitudes using a cross-correlation technique. In particular, we compare the observed emission in 15 selected sky regions to three 'standard' templates. The free-free emission of the diffuse ionized gas is fitted by a well-known spectrum at K and Ka band, but the derived emissivity corresponds to a mean electron temperature of similar to 4000-5000 K. This is inconsistent with estimates from Galactic H II regions although a variation in the derived ratio of H alpha to free-free intensity by a factor of similar to 2 is also found from region to region. The origin of the discrepancy is unclear. The anomalous emission associated with dust is clearly detected in most of the 15 fields studied. The anomalous emission correlates well with the Finkbeiner, Davis & Schlegel model 8 predictions (FDS8) at 94 GHz, with an effective spectral index between 20 and 60 GHz, of beta similar to -2.85. Furthermore, the emissivity varies by a factor of similar to 2 from cloud to cloud. A modestly improved fit to the anomalous dust at K band is provided by modulating the template by an estimate of the dust colour temperature, specifically FDS8 x T-n. We find a preferred value n similar to 1.6, although there is a scatter from region to region. Nevertheless, the preferred index drops to zero at higher frequencies where the thermal dust emission dominates. The synchrotron emission steepens between GHz frequencies and the WMAP bands. There are indications of spectral index variations across the sky but the current data are not precise enough to accurately quantify this from region to region. Our analysis of the WMAP data indicates strongly that the dust-correlated emission at the low WMAP frequencies has a spectrum which is compatible with spinning dust; we find no evidence for a synchrotron component correlated with dust. The importance of these results for the correction of cosmic microwave background data for Galactic foreground emission is discussed. C1 Univ Manchester, Jodrell Bank Observ, Macclesfield SK11 9DL, Cheshire, England. CALTECH, Dept Astron, Pasadena, CA 91125 USA. Max Planck Inst Astrophys, D-85741 Garching, Germany. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. Univ Warsaw Observ, PL-00478 Warsaw, Poland. RP Davies, RD (reprint author), Univ Manchester, Jodrell Bank Observ, Macclesfield SK11 9DL, Cheshire, England. EM rdd@jb.man.ac.uk; cdickins@astro.caltech.edu; banday@MPA-Garching.mpg.de; tjaffe@mpa-garching.mpg.de NR 52 TC 87 Z9 88 U1 0 U2 1 PU BLACKWELL PUBLISHING PI OXFORD PA 9600 GARSINGTON RD, OXFORD OX4 2DQ, OXON, ENGLAND SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD AUG 11 PY 2006 VL 370 IS 3 BP 1125 EP 1139 DI 10.1111/j.1365-2966.2006.10572.x PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 067XR UT WOS:000239336400003 ER PT J AU Babbedge, TSR Rowan-Robinson, M Vaccari, M Surace, JA Lonsdale, CJ Clements, DL Fang, F Farrah, D Franceschini, A Gonzalez-Solares, E Hatziminaoglou, E Lacey, CG Oliver, S Onyett, N Perez-Fournon, I Polletta, M Pozzi, F Rodighiero, G Shupe, DL Siana, B Smith, HE AF Babbedge, T. S. R. Rowan-Robinson, M. Vaccari, M. Surace, J. A. Lonsdale, C. J. Clements, D. L. Fang, F. Farrah, D. Franceschini, A. Gonzalez-Solares, E. Hatziminaoglou, E. Lacey, C. G. Oliver, S. Onyett, N. Perez-Fournon, I. Polletta, M. Pozzi, F. Rodighiero, G. Shupe, D. L. Siana, B. Smith, H. E. TI Luminosity functions for galaxies and quasars in the Spitzer wide-area infrared extragalactic legacy survey SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Review DE galaxies : evolution; galaxies : photometry; quasars : general; cosmology : observations ID HUBBLE-DEEP-FIELD; STAR-FORMATION RATE; DIGITAL-SKY-SURVEY; SPECTRAL ENERGY-DISTRIBUTIONS; ACTIVE GALACTIC NUCLEI; BACKGROUND EXPERIMENT SEARCH; PHOTOMETRIC REDSHIFT CODE; SHAPLEY-AMES GALAXIES; FORMATION HISTORY; SPACE-TELESCOPE AB We construct rest-frame luminosity functions (LFs) at 3.6, 4.5, 5.8, 8 and 24 mu m over the redshift range 0 < z < 2 for galaxies and 0 < z < 4 for optical quasi-stellar objects (QSOs), using optical and infrared (IR) data from the Spitzer Wide-area Infrared Extragalactic (SWIRE) Survey. The 3.6- and 4.5-mu m galaxy LFs show evidence for moderate positive luminosity evolution up to z similar to 1.5, consistent with the passive ageing of evolved stellar populations. Their comoving luminosity density was found to evolve passively, gradually increasing out to z similar to 0.5 - 1 but flattening, or even declining, at higher redshift. Conversely, the 24-mu m galaxy LF, which is more sensitive to obscured star formation and/or active galactic nuclei (AGN) activity, undergoes strong positive evolution, with the derived IR energy density and star formation rate (SFR) density proportional to (1 + z)(gamma) with gamma = 4.5(-0.6)(+0.7) and the majority of this evolution occurring since z similar to 1. Optical QSOs, however, show positive luminosity evolution in all bands, out to the highest redshifts (3 < z < 4). Modelling as L* proportional to ( 1 + z)(gamma) gave gamma = 1.3(-0.1)(+0.1) at 3.6 mu m, gamma = 1.0(-0.1)(+0.1) at 4.5 mu m and stronger evolution at the longer wavelengths (5.8, 8 and 24 mu m), of gamma similar to 3. Comparison of the galaxy LFs to predictions from a semi-analytic model based on cold dark matter (CDM) indicates that an initial mass function (IMF) skewed towards higher mass star formation in bursts compared to locally be preferred. As a result, the currently inferred massive SFRs in distant submm sources may require substantial downwards revision. C1 Univ London Imperial Coll Sci Technol & Med, Astrophys Grp, Blackett Lab, London SW7 2BW, England. CALTECH, Jet Prop Lab, Spitzer Sci Ctr, Pasadena, CA 91125 USA. CALTECH, Jet Prop Lab, Ctr Infrared Proc & Anal, Pasadena, CA 91125 USA. Univ Calif San Diego, Ctr Astrophys & Space Sci, La Jolla, CA 92093 USA. Cornell Univ, Dept Astron, Ithaca, NY 14853 USA. Univ Padua, Dipartimento Astron, Vicolo Osserv, I-35122 Padua, Italy. Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. Inst Astrofis Canarias, E-38200 San Cristobal la Laguna, Spain. Univ Durham, Dept Computat Cosmol, Durham DH1 3LE, England. Univ Sussex, Dept Phys & Astron, Ctr Astron, Brighton BN1 9QH, E Sussex, England. Univ Bologna, Dipartimento Astron, I-40127 Bologna, Italy. RP Babbedge, TSR (reprint author), Univ London Imperial Coll Sci Technol & Med, Astrophys Grp, Blackett Lab, Prince Consort Rd, London SW7 2BW, England. EM thomas.babbedge@imperial.ac.uk RI Vaccari, Mattia/R-3431-2016; OI Vaccari, Mattia/0000-0002-6748-0577; Polletta, Maria del Carmen/0000-0001-7411-5386 NR 127 TC 77 Z9 77 U1 0 U2 0 PU BLACKWELL PUBLISHING PI OXFORD PA 9600 GARSINGTON RD, OXFORD OX4 2DQ, OXON, ENGLAND SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD AUG 11 PY 2006 VL 370 IS 3 BP 1159 EP 1180 DI 10.1111/j.1365-2966.2006.10547.x PG 22 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 067XR UT WOS:000239336400006 ER PT J AU Pope, A Scott, D Dickinson, M Chary, RR Morrison, G Borys, C Sajina, A Alexander, DM Daddi, E Frayer, D MacDonald, E Stern, D AF Pope, Alexandra Scott, Douglas Dickinson, Mark Chary, Ranga-Ram Morrison, Glenn Borys, Colin Sajina, Anna Alexander, David M. Daddi, Emanuele Frayer, David MacDonald, Emily Stern, Daniel TI The Hubble Deep Field-North SCUBA super-map - IV. Characterizing submillimetre galaxies using deep Spitzer imaging SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Review DE galaxies : evolution; galaxies : formation; galaxies : starburst; infrared : galaxies; submillimetre ID STAR-FORMING GALAXIES; ULTRALUMINOUS INFRARED GALAXIES; SPECTRAL ENERGY-DISTRIBUTIONS; REDSHIFT DUSTY GALAXIES; PARKES SELECTED REGIONS; LYMAN BREAK GALAXIES; SPACE-TELESCOPE; RADIO-EMISSION; MIDINFRARED SPECTROSCOPY; SCUBA-8-MJY SURVEY AB We present spectral energy distributions (SEDs), Spitzer colours, and infrared (IR) luminosities for 850-mu m selected galaxies in the Great Observatories Origins Deep Survey Northern (GOODS-N) field. Using the deep Spitzer Legacy images and new data and reductions of the Very Large Array-Hubble Deep Field (VLA-HDF) radio data, we find statistically secure counterparts for 60 per cent (21/35) of our submillimetre (submm) sample, and identify tentative counterparts for another 12 objects. This is the largest sample of submm galaxies with statistically secure counterparts detected in the radio and with Spitzer. Half of the secure counterparts have spectroscopic redshifts, while the other half have photometric redshifts. We find that in most cases the 850-mu m emission is dominated by a single 24-mu m source, with a median flux density of 241 mu Jy, leading to a median 24-to-850-mu m flux density ratio of 0.040. A composite rest-frame SED shows that the submm sources peak at longer wavelengths than those of local ultraluminous infrared galaxies (ULIRGs). Using a basic grey-body model, 850-mu m selected galaxies appear to be cooler than local ULIRGs of the same luminosity. This demonstrates the strong selection effects, both locally and at high redshift, which may lead to an incomplete census of the ULIRG population. The SEDs of submm galaxies are also different from those of their high-redshift neighbours, the near-IR selected BzK galaxies, whose mid-IR-to-radio SEDs are more like those of local ULIRGs. Using 24-mu m, 850-mu m and 1.4-GHz observations, we fit templates that span the mid-IR through radio to derive the integrated IR luminosity (LIR) of the submm galaxies and find a median value of L-IR(8-1000 mu m) = 6.0 x 10(12) L-circle dot. By themselves, 24-mu m and radio fluxes are able to predict L-IR reasonably well because they are relatively insensitive to temperature. However, the submm flux by itself consistently overpredicts L-IR when using spectral templates which obey the local ULIRG temperature-luminosity relation. The shorter Spitzer wavelengths sample the stellar bump at the redshifts of the submm sources, and we find that the Spitzer photometry alone provides a model-independent estimate of the redshift, sigma[Delta z/(1 + z)] = 0.07. The median redshift for our secure submm counterparts is 2.0. Using X-ray and mid-IR data, only 5 per cent of our secure counterparts (1/21) show strong evidence for an active galactic nucleus dominating the LIR. C1 Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada. Natl Opt Astron Observ, Tucson, AZ 85719 USA. Spitzer Sci Ctr, Pasadena, CA 91125 USA. Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. Canada France Hawaii Telescope Corp, Kamuela, HI 96743 USA. CALTECH, Pasadena, CA 91125 USA. Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Pope, A (reprint author), Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada. EM pope@physics.ubc.ca RI Daddi, Emanuele/D-1649-2012; OI Daddi, Emanuele/0000-0002-3331-9590; Scott, Douglas/0000-0002-6878-9840; Alexander, David/0000-0002-5896-6313 NR 104 TC 268 Z9 268 U1 0 U2 3 PU BLACKWELL PUBLISHING PI OXFORD PA 9600 GARSINGTON RD, OXFORD OX4 2DQ, OXON, ENGLAND SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD AUG 11 PY 2006 VL 370 IS 3 BP 1185 EP 1207 DI 10.1111/j.1365-2966.2006.10575.x PG 23 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 067XR UT WOS:000239336400008 ER PT J AU Sansom, AE O'Sullivan, E Forbes, DA Proctor, RN Davis, DS AF Sansom, A. E. O'Sullivan, E. Forbes, Duncan A. Proctor, R. N. Davis, D. S. TI X-ray observations of three young, early-type galaxies SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE galaxies : evolution; galaxies : individual : NGC 4382; galaxies : individual : NGC 5363; galaxies : individual : NGC 2865; galaxies : ISM; X-rays : galaxies ID STELLAR POPULATION-MODELS; ROSAT PSPC OBSERVATIONS; XMM-NEWTON OBSERVATIONS; ELLIPTIC GALAXIES; CHANDRA OBSERVATIONS; FINE-STRUCTURE; HOT GAS; FUNDAMENTAL PLANE; MERGING GALAXIES; STAR-FORMATION AB Massive haloes of hot plasma exist around some, but not all elliptical galaxies. There is evidence that this is related to the age of the galaxy. In this paper, new X-ray observations are presented for three early-type galaxies that show evidence of youth, in order to investigate their X-ray components and properties. NGC 5363 and NGC 2865 were found to have X-ray emission dominated by purely discrete stellar sources. Limits are set on the mass distribution in one of the galaxies observed with XMM - Newton, NGC 4382, which contains significant hot gas. We detect the X-ray emission in NGC 4382 out to 4r(e). The mass-to-light ratio is consistent with a stellar origin in the inner regions but rises steadily to values indicative of some dark matter by 4r(e). These results are set in context with other data drawn from the literature, for galaxies with ages estimated from dynamical or spectroscopic indicators. Ages obtained from optical spectroscopy represent central luminosity-weighted stellar ages. We examine the X-ray evolution with age, normalized by B- and K-band luminosities. Low values of Log( L-X/L-B) and Log( L-X/L-K) are found for all galaxies with ages between 1 and 4 Gyr. Luminous X-ray emission only appears in older galaxies. This suggests that the interstellar medium is removed and then it takes several gigayears for hot gas haloes to build up, following a merger. A possible mechanism for gas expulsion might be associated with feedback from an active nucleus triggered during a merger. C1 Univ Cent Lancashire, Ctr Astrophys, Preston PR1 2HE, Lancs, England. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Swinburne Univ Technol, Ctr Astrophys & Supercomp, Hawthorn, Vic 3122, Australia. Univ Maryland, Joint Ctr Astrophys, Dept Phys, Baltimore, MD 21250 USA. NASA, High Energy Astrophys Lab, Greenbelt, MD 20771 USA. RP Sansom, AE (reprint author), Univ Cent Lancashire, Ctr Astrophys, Preston PR1 2HE, Lancs, England. EM AESansom@uclan.ac.uk OI O'Sullivan, Ewan/0000-0002-5671-6900 NR 76 TC 22 Z9 22 U1 0 U2 1 PU BLACKWELL PUBLISHING PI OXFORD PA 9600 GARSINGTON RD, OXFORD OX4 2DQ, OXON, ENGLAND SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD AUG 11 PY 2006 VL 370 IS 3 BP 1541 EP 1555 DI 10.1111/j.1365-2966.2006.10577.x PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 067XR UT WOS:000239336400037 ER PT J AU Dawson, KS Holzapfel, WL Carlstrom, JE Joy, M LaRoque, SJ AF Dawson, K. S. Holzapfel, W. L. Carlstrom, J. E. Joy, M. LaRoque, S. J. TI Final results from the BIMA CMB anisotropy survey and search for a signature of the Sunyaev-Zel'dovich effect SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmic microwave background; cosmology : observations; galaxies : clusters : general ID MICROWAVE BACKGROUND ANISOTROPY; ANGULAR POWER SPECTRUM; COSMOLOGICAL PARAMETERS; GALAXY CLUSTERS; PROBE; ACBAR; ARRAY AB We report the final results of our study of the cosmic microwave background (CMB) with the BIMA array. Over 1000 hr of observation were dedicated to this project exploring CMB anisotropy, on scales between 10 and 20 in eighteen 6'.6 FWHM fields. In the analysis of the CMB power spectrum, the visibility data are divided into two bins, corresponding to different angular scales. Modeling the observed excess power as a flat band of average multipole l(eff) = 5237, we find Delta T-1(2) = 220(-120)(+140) mu K-2 at 68% confidence and Delta T-1(2) > 0 mu K-2 with 94.7% confidence. In a second band, with average multipole of l(eff) = 8748, we find Delta T-2(2) consistent with zero and an upper limit of 880 mu K-2 at 95% confidence. An extensive series of tests and supplemental observations with the VLA provide strong evidence against systematic errors or radio point sources being the source of the observed excess power. The dominant source of anisotropy on these scales is expected to be the Sunyaev-Zel'dovich (SZ) effect in a population of distant galaxy clusters. If the excess power is due to the SZ effect, we can place constraints on the normalization of the matter power spectrum sigma(8) = 1.03(-0.29)(+0.20) at 68% confidence. The distribution of pixel fluxes in the BIMA images is found to be consistent with simulated observations of the expected SZ background and rules out instrumental noise or radio sources as the source of the observed excess power, with confidence similar to the detection of excess power. Follow-up optical observations to search for galaxy overdensities anticorrelated with flux in the BIMA images, as might be expected from the SZ effect, proved to be inconclusive. C1 Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA. Univ Chicago, Dept Astron & Astrophys, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA. Univ Chicago, Enrico Fermi Inst, Dept Phys, Chicago, IL 60637 USA. NASA, George C Marshall Space Flight Ctr, Dept Space Sci, Huntsville, AL 35812 USA. RP Dawson, KS (reprint author), Univ Calif Berkeley, Lawrence Berkeley Lab, Berkeley, CA 94720 USA. RI Holzapfel, William/I-4836-2015 NR 21 TC 37 Z9 37 U1 0 U2 3 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD AUG 10 PY 2006 VL 647 IS 1 BP 13 EP 24 DI 10.1086/505172 PN 1 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 072BO UT WOS:000239647800003 ER PT J AU Bonamente, M Joy, MK LaRoque, SJ Carlstrom, JE Reese, ED Dawson, KS AF Bonamente, Massimiliano Joy, Marshall K. LaRoque, Samuel J. Carlstrom, John E. Reese, Erik D. Dawson, Kyle S. TI Determination of the cosmic distance scale from Sunyaev-Zel'dovich effect and chandra X-ray measurements of high-redshift galaxy clusters SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmic microwave background; distance scale; X-rays : galaxies : clusters ID HUBBLE-SPACE-TELESCOPE; MICROWAVE BACKGROUND ANISOTROPY; MEDIUM-SENSITIVITY SURVEY; NEARBY CLUSTERS; RYLE TELESCOPE; RX J1347-1145; DARK ENERGY; RADIO HALO; CL 0016+16; CONSTANT AB We determine the distance to 38 clusters of galaxies in the redshift range 0: 14 <= z <= 0: 89 using X-ray data from Chandra and Sunyaev-Zeldovich effect (SZE) data from the Owens Valley Radio Observatory and the Berkeley-Illinois-Maryland Association interferometric arrays. The cluster plasma and dark matter distributions are analyzed using a hydrostatic equilibrium model that accounts for radial variations in density, temperature, and abundance, and the statistical and systematic errors of this method are quantified. The analysis is performed via a Markov chain Monte Carlo technique that provides simultaneous estimation of all model parameters. We measure a Hubble constant of H-0 = 76.9(-3.4)(+3.9) (+10.0)(-8.0) km s(-1) Mpc(-1) (statistical followed by systematic uncertainty at 68% confidence) for an Omega(M) = 0.3, Omega(Lambda) = 0.7 cosmology. We also analyze the data using an isothermal beta-model that does not invoke the hydrostatic equilibrium assumption and find H-0 = 73:7(-3.8)(+4.6) (+9.5)(-7.6) km s(-1) Mpc(-1); to avoid effects from cool cores in clusters, we repeated this analysis excluding the central 100 kpc from the X-ray data and find H-0 = 77.6(-4.3)(+4.8) (+10.1)(-8.2) km s(-1) Mpc(-1) (statistical followed by systematic uncertainty at 68% confidence). The consistency between the models illustrates the relative insensitivity of SZE/X-ray determinations of H-0 to the details of the cluster model. Our determination of the Hubble parameter in the distant universe agrees with the recent measurement from the Hubble Space Telescope Key Project that probes the nearby universe. C1 NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA. Univ Alabama, Dept Phys, Huntsville, AL 35899 USA. Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA. Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA. Univ Chicago, Dept Phys, Chicago, IL 60637 USA. Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA. Univ Calif Davis, Dept Phys, Davis, CA 95616 USA. Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA. RP Bonamente, M (reprint author), NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA. NR 88 TC 191 Z9 192 U1 0 U2 3 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD AUG 10 PY 2006 VL 647 IS 1 BP 25 EP 54 DI 10.1086/505291 PN 1 PG 30 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 072BO UT WOS:000239647800004 ER PT J AU Way, MJ Srivastava, AN AF Way, M. J. Srivastava, A. N. TI Novel methods for predicting photometric redshifts from broadband photometry using virtual sensors SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : distances and redshifts ID DIGITAL SKY SURVEY; ARTIFICIAL NEURAL-NETWORKS; GALAXY-EVOLUTION-EXPLORER; EARLY DATA RELEASE; HUBBLE DEEP FIELD; SURFACE BRIGHTNESS; OPTICAL-PROPERTIES; CATALOG; SDSS; ULTRAVIOLET AB We calculate photometric redshifts from the Sloan Digital Sky Survey Main Galaxy Sample, the Galaxy Evolution Explorer All Sky Survey, and the Two Micron All Sky Survey using two new training-set methods. We utilize the broadband photometry from the three surveys alongside Sloan Digital Sky Survey measures of photometric quality and galaxy morphology. Our first training-set method draws from the theory of ensemble learning while the second employs Gaussian process regression, both of which allow for the estimation of redshift along with a measure of uncertainty in the estimation. The Gaussian process models the data very effectively with small training samples of approximately 1000 points or less. These two methods are compared to a well-known artificial neural network training-set method and to simple linear and quadratic regression. We also demonstrate the need to provide confidence bands on the error estimation made by both classes of models. Our results indicate that variations due to the optimization procedure used for almost all neural networks, combined with the variations due to the data sample, can produce models with variations in accuracy that span an order of magnitude. A key contribution of this paper is to quantify the variability in the quality of results as a function of model and training sample. We show how simply choosing the ''best'' model given a data set and model class can produce misleading results. C1 NASA, Ames Res Ctr, Div Space Sci, Moffett Field, CA 94035 USA. NASA, Ames Res Ctr, Intelligent Syst Div, Moffett Field, CA 94035 USA. RP Way, MJ (reprint author), NASA, Ames Res Ctr, Div Space Sci, MS 245-6, Moffett Field, CA 94035 USA. RI Way, Michael/D-5254-2012; OI Way, Michael/0000-0003-3728-0475 NR 56 TC 38 Z9 38 U1 0 U2 3 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD AUG 10 PY 2006 VL 647 IS 1 BP 102 EP 115 DI 10.1086/505293 PN 1 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 072BO UT WOS:000239647800009 ER PT J AU Bregman, JN Temi, P Bregman, JD AF Bregman, Joel N. Temi, Pasquale Bregman, Jesse D. TI The ages of elliptical galaxies from infrared spectral energy distributions SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : elliptical and lenticular, cD; galaxies : ISM; infrared : galaxies; infrared : ISM ID SPITZER-SPACE-TELESCOPE; STELLAR POPULATION HISTORIES; STAR-FORMATION; MIDINFRARED EMISSION; ORBITAL STRUCTURE; INTERMEDIATE-AGE; SPECTROGRAPH IRS; NUCLEAR-DATA; DEEP-FIELD; EVOLUTION AB The mean ages of early-type galaxies obtained from the analysis of optical spectra give a mean age of 8 Gyr at z = 0, with 40% being younger than 6 Gyr. Independent age determinations are possible by using infrared spectra (5-21 mu m), which we have obtained with the Infrared Spectrograph on Spitzer. This age indicator is based on the collective mass-loss rate of stars, in which mass loss from AGB stars produces a silicate emission feature at 9-12 mu m. This feature decreases more rapidly than the shorter wavelength continuum as a stellar population ages, providing an age indicator. From observations of 30 nearby early-type galaxies, 29 show a spectral energy distribution dominated by stars, and one has significant emission from the ISM and is excluded. The infrared age indicators for the 29 galaxies show them all to be old, with a mean age of about 10 Gyr and a standard deviation of only a few Gyr. This is consistent with the ages inferred from the values of M/L-B, but is inconsistent with the ages derived from the optical line indices, which can be much younger. All of these age indicators are luminosity weighted and should be correlated, even if multiple-age components are considered. The inconsistency indicates that there is a significant problem with either the infrared and the M/L-B ages, which agree, or with the ages inferred from the optical absorption lines. C1 Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. NASA, Ames Res Ctr, Astrophys Branch, Moffett Field, CA 94035 USA. SETI Inst, Mountain View, CA 94043 USA. Univ Western Ontario, Dept Phys & Astron, London, ON N6A 3K7, Canada. RP Bregman, JN (reprint author), Univ Michigan, Dept Astron, 501 E Univ Ave, Ann Arbor, MI 48109 USA. NR 40 TC 35 Z9 35 U1 0 U2 3 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD AUG 10 PY 2006 VL 647 IS 1 BP 265 EP 275 DI 10.1086/505190 PN 1 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 072BO UT WOS:000239647800022 ER PT J AU Cannon, JM Smith, JDT Walter, F Bendo, GJ Calzetti, D Dale, DA Draine, BT Engelbracht, CW Gordon, KD Helou, G Kennicutt, RC Leitherer, C Armus, L Buckalew, BA Hollenbach, DJ Jarrett, TH Li, A Meyer, MJ Murphy, EJ Regan, MW Rieke, GH Rieke, MJ Roussel, H Sheth, K Thornley, MD AF Cannon, John M. Smith, John-David T. Walter, Fabian Bendo, George J. Calzetti, Daniela Dale, Daniel A. Draine, Bruce T. Engelbracht, Charles W. Gordon, Karl D. Helou, George Kennicutt, Robert C., Jr. Leitherer, Claus Armus, Lee Buckalew, Brent A. Hollenbach, David J. Jarrett, Thomas H. Li, Aigen Meyer, Martin J. Murphy, Eric J. Regan, Michael W. Rieke, George H. Rieke, Marcia J. Roussel, Helene Sheth, Kartik Thornley, Michele D. TI Warm dust and spatially variable polycyclic aromatic hydrocarbon emission in the dwarf starburst galaxy NGC 1705 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : dwarf; galaxies : individual (NGC 1705); galaxies : irregular; galaxies : ISM; infrared : galaxies ID SMALL-MAGELLANIC-CLOUD; STAR-FORMING GALAXIES; SPECTRAL ENERGY-DISTRIBUTIONS; VIRGO CLUSTER GALAXIES; INFRARED-EMISSION; NEARBY GALAXIES; INTERSTELLAR DUST; RADIO-CONTINUUM; NGC 1705; CHANDRA OBSERVATIONS AB We present Spitzer observations of the nearby dwarf starburst galaxy NGC 1705 obtained as part of the Spitzer Infrared Nearby Galaxies Survey. The galaxy morphology is very different shortward and longward of similar to 5 mu m: optical and short-wavelength IRAC imaging shows an underlying red stellar population, with the central super star cluster (SSC) dominating the luminosity; longer wavelength IRAC and MIPS imaging reveals warm dust emission arising from two off-nuclear regions that are offset by similar to 250 pc from the SSC and that dominate the far-IR flux of the system. These regions show little extinction at optical wavelengths. The galaxy has a relatively low global dust mass (similar to 2 x 10(5) M-circle dot, implying a global dust-to-gas mass ratio similar to 2-4 times lower than the Milky Way average, roughly consistent with the metallicity decrease). The off-nuclear dust emission appears to be powered by photons from the same stellar population responsible for the excitation of the observed H alpha emission; these photons are unassociated with the SSC (although a contribution from embedded sources to the IR luminosity of the off-nuclear regions cannot be ruled out). Low-resolution IRS spectroscopy shows moderate-strength PAH emission in the 11.3 mu m band in the more luminous eastern peak; no PAH emission is detected in the SSC or the western dust emission complex. There is significant diffuse emission in the IRAC 8 mu m band after starlight has been removed by scaling shorter wavelength data; the fact that IRS spectroscopy shows spatially variable PAH emission strengths compared to the local continuum within this diffuse gas suggests caution in the interpretation of IRAC diffuse 8 mu m emission as arising from PAH carriers alone. The nebular metallicity of NGC 1705 falls at the transition level of similar to 0.35 Z(circle dot) found by Engelbracht and collaborators, below which PAH emission is difficult to detect; the fact that a system at this metallicity shows spatially variable PAH emission demonstrates the complexity of interpreting diffuse 8 mu m emission in galaxies. NGC 1705 deviates significantly from the canonical far-infrared versus radio correlation, having significant far-infrared emission but no detected radio continuum. C1 Max Planck Inst Astron, D-69117 Heidelberg, Germany. Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. Univ London Imperial Coll Sci Technol & Med, Blackett Lab, Astrophys Grp, London SW7 2AZ, England. Space Telescope Sci Inst, Baltimore, MD 21218 USA. Univ Wyoming, Dept Phys & Astron, Laramie, WY 82071 USA. Princeton Univ Observ, Princeton, NJ 08544 USA. CALTECH, Pasadena, CA 91101 USA. Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. CALTECH, Pasadena, CA 91191 USA. NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. Univ Missouri, Dept Phys & Astron, Columbia, MO 65211 USA. Yale Univ, Dept Astron, New Haven, CT 06520 USA. Bucknell Univ, Dept Phys & Astron, Lewisburg, PA 17837 USA. RP Cannon, JM (reprint author), Wesleyan Univ, Dept Astron, Middletown, CT 06459 USA. EM cannon@astro.wesleyan.edu; jdsmith@as.arizona.edu; walter@mpia.de; g.bendo@imperial.ac.uk; calzetti@stsci.edu; ddale@uwyo.edu; draine@astro.princeton.edu; chad@as.arizona.edu; kgordon@as.arizona.edu; gxh@ipac.caltech.edu; robk@ast.cam.ac.uk; leitherer@stsci.edu; lee@ipac.caltech.edu; brentb@ipac.caltech.edu; hollenba@ism.arc.nasa.gov; jarrett@ipac.caltech.edu; lia@missouri.edu; martinm@stsci.edu; murphy@astro.yale.edu; mregan@stsci.edu; grieke@as.arizona.edu; mrieke@as.arizona.edu; hroussel@irastro.caltech.edu; katrik@astro.caltech.edu; mthornle@bucknell.edu OI Draine, Bruce/0000-0002-0846-936X NR 66 TC 37 Z9 37 U1 0 U2 4 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD AUG 10 PY 2006 VL 647 IS 1 BP 293 EP 302 DI 10.1086/505339 PN 1 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 072BO UT WOS:000239647800024 ER PT J AU Snyder, LE Hollis, JM Jewell, PR Lovas, FJ Remijan, A AF Snyder, L. E. Hollis, J. M. Jewell, P. R. Lovas, F. J. Remijan, A. TI Confirmation of interstellar methylcyanodiacetylene (CH3C5N) SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM : abundances; ISM : clouds; ISM : individual (TMC-1); ISM : molecules; radio lines : ISM ID MOLECULAR CLOUD-1 TMC-1; HYDROCARBON CHEMISTRY; MICROWAVE-SPECTRA; PHYSICS AB Ten spectral lines of the symmetric-top molecule methylcyanodiacetylene (CH3C5N) have been detected with the 100 m Green Bank Telescope (GBT) toward the Taurus molecular cloud TMC-1. Both K = 0 and 1 components of the 12, K-11, K, 13, K-12, K, 14, K-13, K, 15, K-14, K, and 16, K-15, K transitions were observed. Consistent with similar to 10 K kinetic temperature for the TMC-1 dark dust cloud, no higher K-components were detected. The CH3C5N spectra confirm an earlier identification report based on data obtained with the MPIfR 100 m telescope by Snyder and colleagues over 20 years ago. Methyl cyanide (CH3CN), methylcyanoacetylene (CH3C3N), and methylcyanodiacetylene all are found in TMC-1 in decreasing relative abundance, suggesting that simple carbon addition on grains may be possible even in dark clouds. However, the correct formation mechanism for CH3C5N is still not known to within several orders of magnitude. C1 Univ Illinois, Dept Astron, Urbana, IL 61801 USA. NASA, Goddard Space Flight Ctr, Space & Earth Data Comp Div, Greenbelt, MD 20771 USA. Natl Radio Astron Observ, Charlottesville, VA 22903 USA. Natl Inst Stand & Technol, Opt Technol Div, Gaithersburg, MD 20899 USA. RP Snyder, LE (reprint author), Univ Illinois, Dept Astron, 1002 W Green St, Urbana, IL 61801 USA. NR 31 TC 25 Z9 25 U1 0 U2 15 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD AUG 10 PY 2006 VL 647 IS 1 BP 412 EP 417 DI 10.1086/505323 PN 1 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 072BO UT WOS:000239647800035 ER PT J AU Monnier, JD Berger, JP Millan-Gabet, R Traub, WA Schloerb, FP Pedretti, E Benisty, M Carleton, NP Haguenauer, P Kern, P Labeye, P Lacasse, MG Malbet, F Perraut, K Pearlman, M Zhao, M AF Monnier, J. D. Berger, J. -P. Millan-Gabet, R. Traub, W. A. Schloerb, F. P. Pedretti, E. Benisty, M. Carleton, N. P. Haguenauer, P. Kern, P. Labeye, P. Lacasse, M. G. Malbet, F. Perraut, K. Pearlman, M. Zhao, M. TI Few skewed disks found in first closure-phase survey of herbig Ae/Be stars SO ASTROPHYSICAL JOURNAL LA English DT Review DE accretion, accretion disks; binaries : spectroscopic; instrumentation : interferometers; stars : individual (AB Aur, HD 45677, HD 144432; MWC 166, MWC 275, MWC 297, MWC 342, MWC 361; MWC 480, MWC 614, MWC 863, MWC 1080, RY Tau; v1295 Aql); stars : pre-main-sequence; techniques : interferometric ID T-TAURI STARS; YOUNG STELLAR OBJECTS; MAIN-SEQUENCE STARS; KECK INTERFEROMETER OBSERVATIONS; BASE-LINE INTERFEROMETRY; INTERMEDIATE-MASS STARS; OPTICAL INTERFEROMETRY; PROTOPLANETARY DISKS; VERTICAL STRUCTURE; ACCRETION DISKS AB Using the three-telescope IOTA interferometer on Mount Hopkins, we report results from the first near-infrared (lambda = 1.65 mu m) closure-phase survey of young stellar objects (YSOs). These closure phases allow us to unambiguously detect departures from centrosymmetry (i.e., skew) in the emission pattern from YSO disks on the scale of similar to 4 mas, expected from generic "flared disk'' models. Six of 14 targets showed small, yet statistically significant nonzero closure phases, with largest values from the young binary system MWC 361-A and the (pre-main-sequence?) Be star HD 45677. Our observations are quite sensitive to the vertical structure of the inner disk, and we confront the predictions of the "puffed-up inner wall'' models of Dullemond, Dominik, & Natta (DDN). Our data support disk models with curved inner rims because the expected emission appears symmetrically distributed around the star over a wide range of inclination angles. In contrast, our results are incompatible with the models possessing vertical inner walls because they predict extreme skewness (i.e., large closure phases) from the near-IR disk emission that is not seen in our data. In addition, we also present the discovery of mysterious H-band "halos'' (similar to 5%-10% of light on scales 0."01-0."50) around a few objects, a preliminary "parametric imaging'' study for HD 45677, and the first astrometric orbit for the young binary MWC 361-A. C1 Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. Lab Astrophys Grenoble, F-38400 St Martin Dheres, France. CALTECH, Michelson Sci Ctr, Pasadena, CA USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. CALTECH, Jet Prop Lab, Pasadena, CA USA. Univ Massachusetts, Amherst, MA 01003 USA. Alcatel Space Ind, Cannes, France. CEA, LETI, Grenoble, France. RP Monnier, JD (reprint author), Univ Michigan, Dept Astron, 941 Dennison Bldg, Ann Arbor, MI 48109 USA. EM monnier@umich.edu NR 101 TC 97 Z9 98 U1 0 U2 4 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD AUG 10 PY 2006 VL 647 IS 1 BP 444 EP 463 DI 10.1086/505340 PN 1 PG 20 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 072BO UT WOS:000239647800038 ER PT J AU Levan, A Fruchter, A Rhoads, J Mobasher, B Tanvir, N Gorosabel, J Rol, E Kouveliotou, C Dell'Antonio, I Merrill, M Bergeron, E Ceron, JM Masetti, N Vreeswijk, P Antonelli, A Bersier, D Castro-Tirado, A Fynbo, J Garnavich, P Holland, S Hjorth, J Nugent, P Pian, E Smette, A Thomsen, B Thorsett, SE Wijers, R AF Levan, Andrew Fruchter, Andrew Rhoads, James Mobasher, Bahram Tanvir, Nial Gorosabel, Javier Rol, Evert Kouveliotou, Chryssa Dell'Antonio, Ian Merrill, Michael Bergeron, Eddie Castro Ceron, Jose Maria Masetti, Nicola Vreeswijk, Paul Antonelli, Angelo Bersier, David Castro-Tirado, Alberto Fynbo, Johan Garnavich, Peter Holland, Stephen Hjorth, Jens Nugent, Peter Pian, Elena Smette, Alain Thomsen, Bjarne Thorsett, Stephen E. Wijers, Ralph TI Infrared and optical observations of GRB 030115 and its extremely red host galaxy: Implications for dark bursts SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : high-redshift; gamma rays : bursts ID GAMMA-RAY BURSTS; HUBBLE-SPACE-TELESCOPE; X-RAY; STARBURST GALAXIES; DUST EXTINCTION; BAND AFTERGLOW; STAR-FORMATION; BRIGHT; SUBMILLIMETER; SUPERNOVA AB We present near-infrared (NIR) and optical observations of the afterglow of GRB 030115. Discovered in an infrared search at Kitt Peak 5 hr after the burst trigger, this afterglow is the faintest ever observed in the R band at such an early epoch and exhibits very red colors, with R - K approximate to 6. The optical magnitude of the afterglow of GRB 030115 is fainter than many upper limits for other bursts, suggesting that without early NIR observations it would have been classified as a "dark'' burst. Both the color and optical magnitude of the afterglow are likely due to dust extinction at moderate redshift z > 2 and indicate that at least some optical afterglows are very faint due to dust along the line of sight. Multicolor Hubble Space Telescope observations were also taken of the host galaxy and the surrounding field. Photometric redshifts imply that the host and a substantial number of faint galaxies in the field are at z similar to 2.5. The overdensity of galaxies is sufficiently great that GRB 030115 may have occurred in a rich high-redshift cluster. The host galaxy shows extremely red colors (R - K = 5) and is the first GRB host to be classified as an extremely red object (ERO). Some of the galaxies surrounding the host also show very red colors, while the majority of the cluster are much bluer, indicating ongoing unobscured star formation. As it is thought that much of high-redshift star formation occurs in highly obscured environments, it may well be that GRB 030115 represents a transition object, between the relatively unobscured afterglows seen to date and a population of objects that are very heavily extinguished, even in the NIR. C1 Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England. Space Telescope Sci Inst, Baltimore, MD 21218 USA. Univ Hertfordshire, Ctr Astrophys Res, Hatfield AL10 9AB, Herts, England. CSIC, IAA, E-18080 Granada, Spain. Univ Amsterdam, Inst Astron, NL-1098 SJ Amsterdam, Netherlands. NASA, MSFC, NSSTC, Huntsville, AL 35805 USA. Brown Univ, Dept Phys, Providence, RI 02912 USA. Natl Opt Astron Observ, Tucson, AZ 85726 USA. Ist Astrofis Spaziale & Fis Cosm, Sez Bologna, CNR, I-40129 Bologna, Italy. European So Observ, Santiago 19, Chile. Osserv Astron Roma, I-00040 Monte Porzio Catone, Italy. Aarhus Univ, Dept Phys & Astron, DK-8000 Aarhus, Denmark. Univ Notre Dame, Dept Phys, Notre Dame, IN 46556 USA. USN Observ, Flagstaff, AZ 86002 USA. Univ Copenhagen, Astron Observ, DK-2100 Copenhagen, Denmark. Lawrence Berkeley Natl Lab, Berkeley, CA 94720 USA. Osserv Astron Trieste, I-34131 Trieste, Italy. Univ Liege, Inst Astrophys & Geophys, B-4000 Cointe Ougree, Belgium. Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA. RP Levan, A (reprint author), Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England. RI Hjorth, Jens/M-5787-2014; OI Hjorth, Jens/0000-0002-4571-2306; Castro-Tirado, A. J./0000-0003-2999-3563; Masetti, Nicola/0000-0001-9487-7740; Pian, Elena/0000-0001-8646-4858 NR 81 TC 51 Z9 51 U1 0 U2 4 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD AUG 10 PY 2006 VL 647 IS 1 BP 471 EP 482 DI 10.1086/503595 PN 1 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 072BO UT WOS:000239647800040 ER PT J AU Saumon, D Marley, MS Cushing, MC Leggett, SK Roellig, TL Lodders, K Freedman, RS AF Saumon, D. Marley, M. S. Cushing, M. C. Leggett, S. K. Roellig, T. L. Lodders, K. Freedman, R. S. TI Ammonia as a tracer of chemical equilibrium in the T7.5 dwarf gliese 570D SO ASTROPHYSICAL JOURNAL LA English DT Article DE stars : abundances; stars : atmospheres; stars : individual (Gliese 570D); stars : low-mass, brown dwarfs ID LOW-MASS STARS; T-DWARFS; BROWN DWARFS; CARBON-MONOXIDE; GIANT PLANETS; DEEP ATMOSPHERE; SOLAR-SYSTEM; ABUNDANCES; CHEMISTRY; 229B AB We present the first analysis of an optical to mid-infrared spectrum of the T7.5 dwarf Gliese 570D with model atmospheres, synthetic spectra, and brown dwarf evolution sequences. We obtain precise values for the basic parameters of G1 570D: T-eff = 800-820 K, log g (cm s(-2)) 5.09-5.23, and log (L/L-circle dot) = -5.525 to -5.551. The Spitzer Infrared Spectrograph (IRS) spectrum shows prominent features of ammonia (NH3) that can only be fitted by reducing the abundance of NH3 by about 1 order of magnitude from the value obtained with chemical-equilibrium models. We model departures from chemical equilibrium in the atmosphere of Gl 570D by considering the kinetics of nitrogen and carbon chemistry in the presence of vertical mixing. The resulting model spectrum reproduces the data very well. C1 Los Alamos Natl Lab, Los Alamos, NM 87545 USA. NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. Joint Astron Ctr, Hilo, HI 96720 USA. Washington Univ, Dept Earth & Planetary Sci, St Louis, MO 63130 USA. SETI Inst, Mountain View, CA 94043 USA. RP Saumon, D (reprint author), Los Alamos Natl Lab, MS P365, Los Alamos, NM 87545 USA. EM dsaumon@lanl.gov; mark.s.marley@nasa.gov; mcushing@as.arizona.edu; s.leggett@jach.hawaii.edu; thomas.l.roellig@nasa.gov; lodders@levee.wustl.edu; freedman@darkstar.arc.nasa.gov OI Leggett, Sandy/0000-0002-3681-2989 NR 48 TC 110 Z9 110 U1 0 U2 5 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD AUG 10 PY 2006 VL 647 IS 1 BP 552 EP 557 DI 10.1086/505419 PN 1 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 072BO UT WOS:000239647800046 ER PT J AU Riley, P Schatzman, C Cane, HV Richardson, IG Gopalswamy, N AF Riley, Pete Schatzman, C. Cane, H. V. Richardson, I. G. Gopalswamy, N. TI On the rates of coronal mass ejections: Remote solar and in situ observations SO ASTROPHYSICAL JOURNAL LA English DT Article DE solar wind; Sun : activity; Sun : corona; Sun : coronal mass ejections (CMEs); Sun : magnetic fields ID 3-DIMENSIONAL PROPAGATION; MAGNETIC CLOUDS; CYCLE VARIATION; PROMINENCE; STREAMER; DRIVEN; CMES AB We compare the rates of coronal mass ejections (CMEs) as inferred from remote solar observations and interplanetary CMEs (ICMEs) as inferred from in situ observations at both 1 AU and Ulysses from 1996 through 2004. We also distinguish between those ICMEs that contain a magnetic cloud (MC) and those that do not. While the rates of CMEs and ICMEs track each other well at solar minimum, they diverge significantly in early 1998, during the ascending phase of the solar cycle, with the remote solar observations yielding approximately 20 times more events than are seen at 1 AU. This divergence persists through 2004. A similar divergence occurs between MCs and non-MC ICMEs. We argue that these divergences are due to the birth of midlatitude active regions, which are the sites of a distinct population of CMEs, only partially intercepted by Earth, and we present a simple geometric argument showing that the CME and ICME rates are consistent with one another. We also acknowledge contributions from (1) an increased rate of high-latitude CMEs and (2) focusing effects from the global solar field. While our analysis, coupled with numerical modeling results, generally supports the interpretation that whether one observes a MC within an ICME is sensitive to the trajectory of the spacecraft through the ICME (i. e., an observational selection effect), one result directly contradicts it. Specifically, we find no systematic offset between the latitudinal origin of ICMEs that contain MCs at 1 AU in the ecliptic plane and that of those that do not. C1 Sci Applicat Int Corp, San Diego, CA 92121 USA. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Catholic Univ Amer, Ctr Solar Phys & Space Weather, Washington, DC 20064 USA. Univ Tasmania, Sch Math & Phys, Hobart, Tas, Australia. Univ Maryland, Dept Astron, College Pk, MD 20742 USA. RP Riley, P (reprint author), Sci Applicat Int Corp, San Diego, CA 92121 USA. EM pete.riley@saic.com; courtney.schatzman@gmail.com; hilary.cane@utas.edu.au; richardson@lheavx.gsfc.nasa.gov; gopals@fugee.gsfc.nasa.gov RI Gopalswamy, Nat/D-3659-2012; OI Richardson, Ian/0000-0002-3855-3634; Gopalswamy, Nat/0000-0001-5894-9954 NR 34 TC 51 Z9 51 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 AUG 10 PY 2006 VL 647 IS 1 BP 648 EP 653 DI 10.1086/505383 PN 1 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 072BO UT WOS:000239647800057 ER PT J AU Feldman, PD Lupu, RE McCandliss, SR Weaver, HA A'Hearn, MF Belton, MJS Meech, KJ AF Feldman, Paul D. Lupu, Roxana E. McCandliss, Stephan R. Weaver, Harold A. A'Hearn, Michael F. Belton, Michael J. S. Meech, Karen J. TI Carbon monoxide in comet 9P/Tempel 1 before and after the Deep Impact encounter SO ASTROPHYSICAL JOURNAL LA English DT Article DE comets : individual (9P/Tempel 1); ultraviolet : solar system ID NUCLEUS AB One of the goals of the Hubble Space Telescope program to observe periodic comet 9P/Tempel 1 in conjunction with NASA's Deep Impact mission was to study the generation and evolution of the gaseous coma resulting from the impact. For this purpose, the Solar Blind Channel of the Advanced Camera for Surveys was used with the F140LP filter, which is sensitive primarily to the ultraviolet emission (>= 1400 angstrom) from the CO fourth positive system. Following the impact we detected an increase in brightness, which if all due to CO corresponds to 1.5 x 10(31) molecules, or a mass of 6.6 x 10(5) kg, an amount that would normally be produced by 7 - 10 hours of quiescent outgassing from the comet. This number is <= 10% of the number of water molecules excavated and suggests that the volatile content of the material excavated by the impact did not differ significantly from the surface or near-subsurface material responsible for the quiescent outgassing of the comet. C1 Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. Johns Hopkins Univ, Appl Phys Lab, Space Dept, Laurel, MD 20723 USA. Univ Maryland, Dept Astron, College Pk, MD USA. Belton Space Explorat Initiat, Tucson, AZ 85716 USA. NASA Astrobiol Inst, Honolulu, HI 96822 USA. Univ Hawaii, Belton Space Explorat Initiatives, Honolulu, HI 96822 USA. RP Feldman, PD (reprint author), Johns Hopkins Univ, Dept Phys & Astron, 3400 N Charles St, Baltimore, MD 21218 USA. EM pdf@pha.jhu.edu; roxana@pha.jhu.edu; stephan@pha.jhu.edu; hal.weaver@jhuapl.edu; ma@astro.umd.edu; mbelton@dakotacom.net; meech@ifa.hawaii.edu RI Lupu, Roxana/P-9060-2014; Weaver, Harold/D-9188-2016 OI Lupu, Roxana/0000-0003-3444-5908; NR 17 TC 21 Z9 21 U1 0 U2 3 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD AUG 10 PY 2006 VL 647 IS 1 BP L61 EP L64 DI 10.1086/507464 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 072BQ UT WOS:000239648000016 ER PT J AU Neufeld, DA Green, JD Hollenbach, DJ Sonnentrucker, P Melnick, GJ Bergin, EA Snell, RL Forrest, WJ Watson, DM Kaufman, MJ AF Neufeld, David A. Green, Joel D. Hollenbach, David J. Sonnentrucker, Paule Melnick, Gary J. Bergin, Edwin A. Snell, Ronald L. Forrest, William J. Watson, Dan M. Kaufman, Michael J. TI Spitzer observations of hydrogen deuteride SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM : abundances; ISM : clouds; ISM : molecules; molecular processes ID ULTRAVIOLET-SPECTROSCOPIC-EXPLORER; INTERSTELLAR-MEDIUM; ROVIBRATIONAL EXCITATION; MOLECULAR-HYDROGEN; MILKY-WAY; HD; OXYGEN; RATIO; ABSORPTION; DEPLETION AB We report the detection of interstellar hydrogen deuteride (HD) toward the supernova remnant IC 443, and the tentative detection of HD toward the Herbig-Haro objects HH 54 and HH 7 and the star-forming region GGD 37 (Cep A West). Our detections are based upon spectral line mapping observations of the R(3) and R(4) rotational lines of HD, at rest wavelengths of 28.502 and 23.034 mu m, respectively, obtained using the Infrared Spectrograph on board the Spitzer Space Telescope. The HD R(4)/R(3) line intensity ratio promises to be a valuable probe of the gas pressure in regions where it can be observed. The derived HD/H2 abundance ratios are (1.19(-0.24)(+0.35)) x 10(-5), (1.80(-0.32)(+0.54)) x 10(-5), and (1.41(-0.33)(+0.46)) x 10(-5), respectively (68.3% confidence limits, based upon statistical errors alone) for IC 443 (clump C), HH 54, and HH 7. If HD is the only significant reservoir of gas-phase deuterium in these sources, the inferred HD/H-2 ratios are all consistent with a gas-phase elemental abundance [n(D)/n(H)](gas) similar to 7.5 x 10(-6), a factor of 2-3 below the values obtained previously from observations of atomic deuterium in the Local Bubble and the Galactic halo. However, similarly low gas-phase deuterium abundances have been inferred previously for molecular gas clouds in the Orion region and in atomic clouds along sight lines within the Galactic disk to stars more distant than 500 pc from the Sun. C1 Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. Univ Rochester, Dept Phys & Astron, Rochester, NY 14627 USA. NASA Ames Res Ctr, Moffett Field, CA 94035 USA. Harvard Univ, Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Michigan, Dept Astron, Ann Arbor, MI USA. Univ Massachusetts, Dept Astron, Amherst, MA 01003 USA. San Jose State Univ, Dept Phys, San Jose, CA 95192 USA. RP Neufeld, DA (reprint author), Johns Hopkins Univ, Dept Phys & Astron, 3400 N Charles St, Baltimore, MD 21218 USA. NR 27 TC 22 Z9 22 U1 0 U2 4 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD AUG 10 PY 2006 VL 647 IS 1 BP L33 EP L36 DI 10.1086/507130 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 072BQ UT WOS:000239648000009 ER PT J AU Pearson, JC Drouin, BJ AF Pearson, J. C. Drouin, Brian J. TI Laboratory measurement of the J=1-0 transition of CH+ SO ASTROPHYSICAL JOURNAL LA English DT Article DE methods : laboratory; molecular data; radio lines : general ID LASER MAGNETIC-RESONANCE; INTERSTELLAR CLOUDS; BAND SYSTEM; SPECTROSCOPIC ANALYSIS; ROTATIONAL SPECTRUM; ABSORPTION-LINES; EMISSION BANDS; MOLECULES; CONSTANTS; PROFILES AB The A(1)Pi-X-1 Sigma electronic band of the CH+ ion has been used as a probe of the physical and dynamical conditions of the interstellar medium ( ISM) for 65 years. In spite of being one of the first molecular species observed in the ISM, and the very large number of subsequent observations with large derived column densities, the pure rotational spectra of CH+ has remained elusive in both the laboratory and, with one exception (Cernicharo et al.), the ISM as well. We report the first laboratory measurement of the pure rotation of the CH+ ion J = 1-0 at 835078.950(75) MHz. Also reported are the somewhat unexpected chemical conditions that resulted in 1-0 laboratory production. A mass-independent analysis of the existing optical data and the microwave transition is presented, along with predictions for rotational transition frequencies of isotopomers of CH+. C1 CALTECH, Jet Propuls Lab, Pasadena, CA 91109 USA. RP Pearson, JC (reprint author), CALTECH, Jet Propuls Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. NR 43 TC 20 Z9 20 U1 1 U2 4 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD AUG 10 PY 2006 VL 647 IS 1 BP L83 EP L86 DI 10.1086/506522 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 072BQ UT WOS:000239648000021 ER PT J AU Christopher, SA Zhang, JL Kaufman, YJ Remer, LA AF Christopher, Sundar A. Zhang, Jianglong Kaufman, Yoram J. Remer, Lorraine A. TI Satellite-based assessment of top of atmosphere anthropogenic aerosol radiative forcing over cloud-free oceans SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article AB Most assessments of the direct climate forcing (DCF) of anthropogenic aerosols are from numerical simulations. However, recent advances in remote sensing techniques allow the separation of fine mode aerosols ( anthropogenic aerosol is mostly fine aerosol) from coarse mode aerosols ( largely marine and dust, which are mostly natural) from satellite data such as the Moderate Resolution Imaging SpectroRadiometer ( MODIS). Here, by combining MODIS narrowband measurements with broadband radiative flux data sets from the Clouds and the Earth's Radiant Energy System (CERES), we provide a measurement-based assessment of the global direct climate forcing ( DCF) of anthropogenic aerosols at the top of atmosphere (TOA) only for cloud free oceans. The mean TOA DCF of anthropogenic aerosols over cloud-free oceans [60N - 60S] is - 1.4 +/- 0.9 Wm(-2), which is in excellent agreement ( mean value of - 1.4 Wm(-2)) with a recent observational study by Kaufman et al. [ 2005]. C1 Univ Alabama, Dept Atmospher Sci, Huntsville, AL 35806 USA. NASA, Goddard Space Flight Ctr, Atmospheres Lab, Greenbelt, MD 20771 USA. RP Christopher, SA (reprint author), Univ Alabama, Dept Atmospher Sci, 320 Sparkman Dr,NSSTC, Huntsville, AL 35806 USA. EM sundar@nsstc.uah.edu; jianglong.zhang@.nrlmry.navy.mil RI Christopher, Sundar/E-6781-2011 NR 11 TC 35 Z9 35 U1 1 U2 5 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD AUG 10 PY 2006 VL 33 IS 15 AR L15816 DI 10.1029/2005GL025535 PG 4 WC Geosciences, Multidisciplinary SC Geology GA 074BB UT WOS:000239786100001 ER PT J AU Ben-Ze'Ev, E Karnieli, A Agam, N Kaufman, Y Holben, B AF Ben-Ze'Ev, E. Karnieli, A. Agam, N. Kaufman, Y. Holben, B. TI Assessing vegetation condition in the presence of biomass burning smoke by applying the Aerosol-free Vegetation Index (AFRI) on MODIS images SO INTERNATIONAL JOURNAL OF REMOTE SENSING LA English DT Article ID EOS-MODIS; ATMOSPHERIC CORRECTION; OPTICAL-PROPERTIES; REFLECTANCE; TROPICS; AVHRR AB Vegetation indices (VIs) such as the Normalized Difference Vegetation Index (NDVI) are widely used for assessing vegetation cover and condition. One of the NDVI's significant disadvantages is its sensitivity to aerosols in the atmosphere, hence several atmospherically resistant VIs were formulated using the difference in the radiance between the blue and the red spectral bands. The state-of-the-art atmospherically resistant VI, which is a standard Moderate Resolution Imaging Spectroradiometer (MODIS) product, together with the NDVI, is the Enhanced Vegetation Index (EVI). A different approach introduced the Aerosol-free Vegetation Index (AFRI) that is based on the correlation between the shortwave infrared (SWIR) and the visible red bands. The AFRI main advantage is in penetrating an opaque atmosphere influenced by biomass burning smoke, without the need for explicit correction for the aerosol effect. The objective of this research was to compare the performance of these three VIs under smoke conditions. The AFRI was applied to the 2.1 mu m SWIR channel of the MODIS sensor onboard the Earth Observing System (EOS) Terra and Aqua satellites in order to assess its functionality on these imaging platforms. The AFRI performance was compared with those of NDVI and EVI. All VIs were calculated on images with and without present smoke, using the surface-reflectance MODIS product, for three case studies of fires in Arizona, California, and Zambia. The MODIS Fire Product was embedded on the images in order to identify the exact location of the active fires. Although good correlations were observed between all VIs in the absence of smoke (in the Arizona case R-2=0.86, 0.77, 0.88 for the NDVI-EVI, AFRI-EVI, and AFRI-NDVI, respectively) under smoke conditions a high correlation was maintained between the NDVI and the EVI, while low correlations were found for the AFRI-EVI and AFRI-NDVI (0.21 and 0.16, for the Arizona case, respectively). A time series of MODIS images recorded over Zambia during the summer of 2000 was tested and showed high NDVI fluctuations during the study period due to oscillations in aerosol optical thickness values despite application of aerosol corrections on the images. In contrast, the AFRI showed smoother variations and managed to better assess the vegetation condition. It is concluded that, beneath the biomass burning smoke, the AFRI is more effective than the EVI in observing the vegetation conditions. C1 Ben Gurion Univ Negev, Jacob Blaustein Inst Desert Res, Remote Sensing Lab, IL-84990 Sede Boqer, Israel. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Karnieli, A (reprint author), Ben Gurion Univ Negev, Jacob Blaustein Inst Desert Res, Remote Sensing Lab, Sede Boker Campus, IL-84990 Sede Boqer, Israel. EM karnieli@bgu.ac.il OI Agam, Nurit/0000-0002-8921-6179 NR 29 TC 17 Z9 17 U1 1 U2 7 PU TAYLOR & FRANCIS LTD PI ABINGDON PA 4 PARK SQUARE, MILTON PARK, ABINGDON OX14 4RN, OXON, ENGLAND SN 0143-1161 J9 INT J REMOTE SENS JI Int. J. Remote Sens. PD AUG 10 PY 2006 VL 27 IS 15 BP 3203 EP 3221 DI 10.1080/01431160500177380 PG 19 WC Remote Sensing; Imaging Science & Photographic Technology SC Remote Sensing; Imaging Science & Photographic Technology GA 070PG UT WOS:000239534700008 ER PT J AU Liu, Y Vinokur, M Wang, ZJ AF Liu, Y Vinokur, M Wang, ZJ TI Spectral difference method for unstructured grids I: Basic formulation SO JOURNAL OF COMPUTATIONAL PHYSICS LA English DT Article DE high-order; conservation laws; unstructured grids; spectral difference; spectral collocation method ID FINITE VOLUME METHOD; CHEBYSHEV MULTIDOMAIN METHOD; NAVIER-STOKES EQUATIONS; ONE-DIMENSIONAL SYSTEMS; CONSERVATION-LAWS; ELEMENT METHOD; POLYNOMIAL INTERPOLATION; COMPRESSIBLE FLOWS; HYPERBOLIC SYSTEMS; REAL FUNCTIONS AB A new, high-order, conservative, and efficient method for conservation laws on unstructured grids is developed. It combines the best features of structured and unstructured grid methods to attain computational efficiency and geometric flexibility; it utilizes the concept of discontinuous and high-order local representations to achieve conservation and high accuracy; and it is based on the finite-difference formulation for simplicity. Universal reconstructions are obtained by distributing unknown and flux points in a geometrically similar manner for all unstructured cells. Placements of these points with various orders of accuracy are given for the triangular elements. Accuracy studies of the method are carried out with the two-dimensional linear wave equation and Burgers' equation, and each order of accuracy is verified numerically. Numerical solutions of plane electromagnetic waves incident on perfectly conducting circular cylinders are presented and compared with the exact solutions to demonstrate the capability of the method. Excellent agreement has been found. The method is much simpler than the discontinuous Galerkin and spectral volume methods for unstructured grids. (c) 2006 Elsevier Inc. All rights reserved. C1 NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. Eloret Corp, Sunnyvale, CA 94087 USA. Iowa State Univ, Dept Aerosp Engn, Ames, IA 50011 USA. RP Liu, Y (reprint author), NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. EM Yen.Liu@nasa.gov; zjw@iastate.edu RI Wang, Z.J./A-9628-2010 OI Wang, Z.J./0000-0002-6203-6303 NR 44 TC 142 Z9 150 U1 2 U2 13 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 AUG 10 PY 2006 VL 216 IS 2 BP 780 EP 801 DI 10.1016/j.jcp.2006.01.024 PG 22 WC Computer Science, Interdisciplinary Applications; Physics, Mathematical SC Computer Science; Physics GA 057HG UT WOS:000238586300016 ER PT J AU Gutsev, GL Mochena, MD Bauschlicher, CW AF Gutsev, G. L. Mochena, M. D. Bauschlicher, C. W., Jr. TI Structure and Properties of Mn-n, Mn-n(-), and Mn-n(+) clusters (n= 3-10) SO JOURNAL OF PHYSICAL CHEMISTRY A LA English DT Article ID ELECTRONIC POPULATION ANALYSIS; MOLECULAR WAVE FUNCTIONS; DENSITY-FUNCTIONAL THEORY; GAUSSIAN-BASIS SETS; IONIZATION ENERGIES; MANGANESE CLUSTERS; MAGNETIC ORDER; SPIN-RESONANCE; FE-N; TRANSITION AB Electronic and geometrical structures of Mn-3-Mn-10 together with their singly negatively and positively charged ions are computed using density functional theory with generalized gradient approximation. The ground-state spin multiplicities in the neutral series are 16, 21, 4, 9, 6, 5, 2, and 5, for Mn-3-Mn-10, respectively. Thus, there is a transition from a ferromagnetic ground state to a ferrimagnetic ground state at Mn-5. The energy difference between ferrimagnetic and ferromagnetic states in Mn-n grows rapidly with increasing n and exceeds 2 eV in Mn-10. The corresponding change from ferro- to ferrimagnetic ground state occurs at Mn-6(-) and Mn-3(+) in the anionic and cationic series, respectively. Beginning with Mn-6, the ion spin multiplicities differ from that of the neutral by +/- 1 (i.e., they obey the empirical "+/- 1 rule"). We found that the energy required to remove an Mn atom is nearly independent of the charge state of an Mnn cluster and the number of atoms in the cluster, except for Mn-3. The results of our calculations are in reasonable agreement with experiment, except for the experimental data on the magnetic moments per atom, where, in general, we predict smaller values than the experiment. C1 Florida A&M Univ, Dept Phys, Tallahassee, FL 32307 USA. NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Gutsev, GL (reprint author), Florida A&M Univ, Dept Phys, Tallahassee, FL 32307 USA. EM gennady.gutsev@famu.edu NR 50 TC 23 Z9 23 U1 0 U2 11 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 1089-5639 J9 J PHYS CHEM A JI J. Phys. Chem. A PD AUG 10 PY 2006 VL 110 IS 31 BP 9758 EP 9766 DI 10.1021/jp0625331 PG 9 WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical SC Chemistry; Physics GA 069RO UT WOS:000239466100025 PM 16884208 ER PT J AU Kwan, AJ Crounse, JD Clarke, AD Shinozuka, Y Anderson, BE Crawford, JH Avery, MA McNaughton, CS Brune, WH Singh, HB Wennberg, PO AF Kwan, Alan J. Crounse, John D. Clarke, Antony D. Shinozuka, Yohei Anderson, Bruce E. Crawford, James H. Avery, Melody A. McNaughton, Cameron S. Brune, William H. Singh, Hanwant B. Wennberg, Paul O. TI On the flux of oxygenated volatile organic compounds from organic aerosol oxidation SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID ATMOSPHERIC PARTICLES; TROPICAL PACIFIC; TROPOSPHERE; OZONE; O-3; ADSORPTION; ISOPRENE; PRODUCTS; MATTER; FATE AB Previous laboratory and field studies suggest that oxidation of organic aerosols can be a source of oxygenated volatile organic compounds (OVOC). Using measurements of atmospheric oxidants and aerosol size distributions performed on the NASA DC-8 during the INTEX-NA campaign, we estimate the potential magnitude of the continental summertime OVOC flux from organic aerosol oxidation by OH to be as large as similar to 70 pptv C/day in the free troposphere. Contributions from O-3, H2O2, photolysis, and other oxidants may increase this estimate. These processes may provide a large, diffuse source of OVOC that has not been included in current atmospheric models, and thus have a significant impact on our understanding of organic aerosol, OVOC, PAN, and HOx chemistry. The potential importance and highly uncertain nature of our estimate highlights the need for more field and laboratory studies on organic aerosol composition and aging. C1 CALTECH, Div Engn & Appl Sci, Pasadena, CA 91125 USA. CALTECH, Div Chem & Chem Engn, Pasadena, CA 91125 USA. Univ Hawaii Manoa, Dept Oceanog, Honolulu, HI 96822 USA. NASA, Langley Res Ctr, Hampton, VA 23681 USA. Penn State Univ, Dept Meteorol, University Pk, PA 16802 USA. NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. RP Kwan, AJ (reprint author), CALTECH, Div Engn & Appl Sci, Pasadena, CA 91125 USA. EM kwan@caltech.edu RI Crounse, John/E-4622-2011; Wennberg, Paul/A-5460-2012; Crawford, James/L-6632-2013; Crounse, John/C-3700-2014 OI Crawford, James/0000-0002-6982-0934; Crounse, John/0000-0001-5443-729X NR 40 TC 33 Z9 33 U1 0 U2 11 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 EI 1944-8007 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD AUG 9 PY 2006 VL 33 IS 15 AR L15815 DI 10.1029/2006GL026144 PG 5 WC Geosciences, Multidisciplinary SC Geology GA 074BA UT WOS:000239786000004 ER PT J AU Wei, CY AF Wei, Chenyu TI Radius and chirality dependent conformation of polymer molecule at nanotube interface SO NANO LETTERS LA English DT Article ID WALL CARBON NANOTUBE; SHORT-RANGE ORDER; DYNAMICS SIMULATIONS; COMPOSITES; GRAPHITE; PROTEINS; SURFACE; LIQUID; MELTS; DNA AB Temperature-dependent conformations of linear polymer molecules adsorbed at carbon nanotube (CNT) interfaces are investigated through molecule dynamics simulations. Model polyethylene (PE) molecules are shown to have selective conformations on the CNT surface, controlled by atomic structures of the CNT lattice and geometric coiling energy. PE molecules form entropy driven assembly domains, and their preferred wrapping angles around large radius CNT (40, 40) reflect the molecule configurations with energy minimums on a graphite plane. While PE molecules prefer 0 degrees wrapping on small radius armchair CNT (5, 5) predominantly at low temperatures, their configurations are shifted to larger wrapping angle ones on a similar radius zigzag CNT (10, 0). A nematic transformation around 280 K is identified through the Landau - de Gennes theory, with molecule aligning along tube axis in extended conformations. C1 NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Wei, CY (reprint author), NASA, Ames Res Ctr, MS 229-1, Moffett Field, CA 94035 USA. EM cwei@mail.arc.nasa.gov NR 34 TC 63 Z9 64 U1 3 U2 20 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 1530-6984 J9 NANO LETT JI Nano Lett. PD AUG 9 PY 2006 VL 6 IS 8 BP 1627 EP 1631 DI 10.1021/nl0605770 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 071SY UT WOS:000239623900010 PM 16895347 ER PT J AU Xue, CC Meador, MAB Zhu, L Ge, JJ Cheng, SZD Putthanarat, S Eby, RK Khalfan, A Bennett, GD Greenbaum, SG AF Xue, Chenchen Meador, Mary Ann B. Zhu, Lei Ge, Jason J. Cheng, Stephen Z. D. Putthanarat, Sirina Eby, R. K. Khalfan, Ameesh Bennett, George D. Greenbaum, Steve G. TI Morphology of PI-PEO block copolymers for lithium batteries SO POLYMER LA English DT Article DE lithium batteries; solid polymer electrolytes; morphology ID POLYMER ELECTROLYTES; POLY(ETHYLENE OXIDE); TRANSPORT; CRYSTALLIZATION; LAMELLAE AB Polyimide (PI)-polyethylene oxide (PEO) block copolymers have a wide variety of applications in microelectronics, since PI-PEO films exhibit a high degree of thermal and chemical stability. The polymers consist of short, rigid rod T-shaped PI segments, alternating with flexible, PEO coil segments. The highly incompatible PI rods and PEO coils should phase-separate, especially in the presence of lithium ions used as electrolytes for lithium polymer batteries. The rigid rod phase provides a high degree of dimensional stability. In this paper, we provide evidence by DSC that the self-assembled ordered structure of the PI-PEO molecules is formed from concentrated solution rather than the bulk state. Tapping mode AFM and X-ray diffraction are applied to observe the nanodomains in the phase separation of the PI and PEO before and after doping with lithium ions. In addition, we report evidence of the ion transport primary mechanism, in the amorphous phase of the lithium salt-doped PI-PEO block copolymers' multinuclear NMR linewidth, spin-lattice relaxation time, and pulsed field gradient diffusion measurements. (c) 2006 Elsevier Ltd. All rights reserved. C1 NASA, Glenn Res Ctr, Div Mat, Cleveland, OH 44135 USA. Univ Akron, Maurice Morton Inst Polymer Sci, Akron, OH 44325 USA. Univ Connecticut, Inst Mat Sci, Storrs, CT 06269 USA. Univ Connecticut, Dept Chem Engn, Storrs, CT 06269 USA. Univ Dayton, Dayton, OH 45469 USA. CUNY Hunter Coll, Dept Phys, New York, NY 10021 USA. RP Meador, MAB (reprint author), NASA, Glenn Res Ctr, Div Mat, Mail Stop 49-3,21000 Brookpk Rd, Cleveland, OH 44135 USA. EM maryann.meador@nasa.gov; reby@uakron.edu RI Zhu, Lei/C-8754-2013; OI Zhu, Lei/0000-0001-6570-9123; Meador, Mary Ann/0000-0003-2513-7372 NR 22 TC 14 Z9 14 U1 4 U2 41 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 AUG 9 PY 2006 VL 47 IS 17 BP 6149 EP 6155 DI 10.1016/j.polymer.2006.06.024 PG 7 WC Polymer Science SC Polymer Science GA 076QT UT WOS:000239973500017 ER PT J AU Liang, SL Zheng, T Liu, RG Fang, HL Tsay, SC Running, S AF Liang, Shunlin Zheng, Tao Liu, Ronggao Fang, Hongliang Tsay, Si-Chee Running, Steven TI Estimation of incident photosynthetically active radiation from Moderate Resolution Imaging Spectrometer data SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID MODIS ATMOSPHERE PRODUCTS; SOLAR-RADIATION; SATELLITE DATA; MULTIPLE-SCATTERING; LAND MODEL; SURFACE; PAR; CLIMATE; SCALE; REFLECTANCE AB [ 1] Incident photosynthetically active radiation ( PAR) is a key variable needed by almost all terrestrial ecosystem models. Unfortunately, the current incident PAR products estimated from remotely sensed data at spatial and temporal resolutions are not sufficient for carbon cycle modeling and various applications. In this study, the authors develop a new method based on the look-up table approach for estimating instantaneous incident PAR from the polar-orbiting Moderate Resolution Imaging Spectrometer (MODIS) data. Since the top-of-atmosphere (TOA) radiance depends on both surface reflectance and atmospheric properties that largely determine the incident PAR, our first step is to estimate surface reflectance. The approach assumes known aerosol properties for the observations with minimum blue reflectance from a temporal window of each pixel. Their inverted surface reflectance is then interpolated to determine the surface reflectance of other observations. The second step is to calculate PAR by matching the computed TOA reflectance from the look-up table with the TOA values of the satellite observations. Both the direct and diffuse PAR components, as well as the total shortwave radiation, are determined in exactly the same fashion. The calculation of a daily average PAR value from one or two instantaneous PAR values is also explored. Ground measurements from seven FLUXNET sites are used for validating the algorithm. The results indicate that this approach can produce reasonable PAR product at 1 km resolution and is suitable for global applications, although more quantitative validation activities are still needed. C1 Univ Maryland, Dept Geog, College Pk, MD 20742 USA. Chinese Acad Sci, Inst Geog Sci & Nat Resources Res, Beijing 100101, Peoples R China. NASA, Goddard Space Flight Ctr, Climate & Radiat Branch, Greenbelt, MD 20771 USA. Univ Montana, Sch Forestry, Missoula, MT 59812 USA. RP Liang, SL (reprint author), Univ Maryland, Dept Geog, College Pk, MD 20742 USA. EM sliang@geog.umd.edu RI Tsay, Si-Chee/J-1147-2014; liang, shunlin/C-2809-2015 NR 44 TC 78 Z9 84 U1 3 U2 21 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD AUG 8 PY 2006 VL 111 IS D15 AR D15208 DI 10.1029/2005JD006730 PG 13 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 074BI UT WOS:000239786800006 ER PT J AU Harry, GM Fritschel, P Shaddock, DA Folkner, W Phinney, ES AF Harry, Gregory M. Fritschel, Peter Shaddock, Daniel A. Folkner, William Phinney, E. Sterl TI Laser interferometry for the Big Bang Observer SO CLASSICAL AND QUANTUM GRAVITY LA English DT Article ID MECHANICAL LOSS; STABILIZATION; LIGO AB The Big Bang Observer is a proposed space-based gravitational-wave detector intended as a follow on mission to the Laser Interferometer Space Antenna ( LISA). It is designed to detect the stochastic background of gravitational waves from the early universe. We discuss how the interferometry can be arranged between three spacecraft for this mission and what research and development on key technologies are necessary to realize this scheme. C1 MIT, LIGO Lab, Cambridge, MA 02139 USA. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. CALTECH, Pasadena, CA 91125 USA. RP Harry, GM (reprint author), MIT, LIGO Lab, NW17-161, Cambridge, MA 02139 USA. EM gharry@ligo.mit.edu RI Shaddock, Daniel/A-7534-2011 OI Shaddock, Daniel/0000-0002-6885-3494 NR 13 TC 60 Z9 61 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 AUG 7 PY 2006 VL 23 IS 15 BP 4887 EP 4894 DI 10.1088/0264-9381/23/15/008 PG 8 WC Astronomy & Astrophysics; Physics, Multidisciplinary; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA 069AK UT WOS:000239416800008 ER PT J AU Streets, DG Wu, Y Chin, M AF Streets, David G. Wu, Ye Chin, Mian TI Two-decadal aerosol trends as a likely explanation of the global dimming/brightening transition SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID SURFACE SOLAR-RADIATION; CARBON EMISSIONS; ART.; REDUCTIONS; INVENTORY; BLACK AB Global average trends in solar radiation reaching the Earth's surface show a transition from dimming to brightening that occurred in about 1990. We show that the inter-annual trend in solar radiation between 1980 and 2000 mirrors the trend in primary emissions of SO2 and black carbon, which together contribute about one-third of global average aerosol optical depth. Combined global emissions of these two species peaked in 1988 - 1989. The two-decadal rate of decline in aerosol loading resulting from these emission changes, 0.13% yr(-1), can be compared with the reported increase in solar radiation of 0.10% yr(-1) in 1983 - 2001. Regional patterns of aerosol and radiation changes are also qualitatively consistent. We conclude that changes in the aerosol burden due to changing patterns of anthropogenic emissions are likely contributing to the trends in surface solar radiation. C1 Argonne Natl Lab, Decis & Informat Sci Div, Argonne, IL 60439 USA. Argonne Natl Lab, Div Energy Syst, Argonne, IL 60439 USA. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Streets, DG (reprint author), Argonne Natl Lab, Decis & Informat Sci Div, DIS-900,9700 S Cass Ave, Argonne, IL 60439 USA. EM dstreets@anl.gov RI Chin, Mian/J-8354-2012; Wu, Ye/O-9779-2015; OI Streets, David/0000-0002-0223-1350 NR 20 TC 145 Z9 155 U1 3 U2 39 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 EI 1944-8007 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD AUG 5 PY 2006 VL 33 IS 15 AR L15806 DI 10.1029/2006GL026471 PG 4 WC Geosciences, Multidisciplinary SC Geology GA 071JG UT WOS:000239597000006 ER PT J AU Devasahayam, S Hill, DJT Connell, JW AF Devasahayam, S Hill, DJT Connell, JW TI FT-Raman studies of a range of polyimides subjected to high-energy Radiations at room and elevated temperatures SO JOURNAL OF APPLIED POLYMER SCIENCE LA English DT Article DE FT-Raman; transparent polyimides; e-beam radiolysis; degradation ID ELECTRON-BEAM IRRADIATION; AROMATIC POLYMERS; DEGRADATION; RESISTANCE; RADIOLYSIS; CHEMISTRY; ULTEM AB A range of polyimides have been subjected to electron beam radiolysis at different temperatures. These polyimides were chemically designed to suit space applications, being either transparent or having groups which provide oxidation resistance. The structural changes that occur in the polyimides, when subjected to electron beam irradiation doses up to 18.5 MGy and up to temperatures close to their glass transition temperatures, were studied using FT-Raman spectroscopy. The range of polyimides studied included a series of perfluoropolyimides, a silicon-modified polyimide, and Ultem. The changes in the Raman peak intensities of the different groups indicated scission reactions involving the imide rings and ether linkages. (c) 2006 Wiley Periodicals, Inc. C1 Univ Sydney, Sch Phys, Sydney, NSW 2006, Australia. Univ Queensland, Polymer Mat & Radiat Grp, Dept Chem, Brisbane, Qld 4072, Australia. NASA, Langley Res Ctr, Hampton, VA 23681 USA. RP Devasahayam, S (reprint author), Univ Sydney, Sch Phys, Sydney, NSW 2006, Australia. EM sheila.devasahayam@measurernent.gov.au NR 23 TC 2 Z9 2 U1 2 U2 9 PU JOHN WILEY & SONS INC PI HOBOKEN PA 111 RIVER ST, HOBOKEN, NJ 07030 USA SN 0021-8995 J9 J APPL POLYM SCI JI J. Appl. Polym. Sci. PD AUG 5 PY 2006 VL 101 IS 3 BP 1575 EP 1582 DI 10.1002/app.23547 PG 8 WC Polymer Science SC Polymer Science GA 058AU UT WOS:000238637300045 ER PT J AU Mishin, EV Khazanov, GV AF Mishin, E. V. Khazanov, G. V. TI Tether-induced airglow: Collisionless effects SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID IONOSPHERIC HEATING EXPERIMENTS; UPPER HYBRID; IONIZATION; TURBULENCE; WAVE; ELECTRONS; EISCAT; LAYERS AB A specially-designed sounding rocket experiment with a bare, conducting tether was recently suggested to test an idea that tether-produced energetic-electron beams can be used for remote sensing the neutral density in the E region. This letter contains the theoretical analysis of collisionless beam-plasma interactions (BPI) that complement direct impact of the energetic electrons with neutral particles. Collisionless effects are shown to play a significant and even major role in tether-induced aurora (TA). In the F region, BPI lead to appreciable green-line (557.7 nm) emissions at similar to 200 km. Farther downward, BPI develop inside a local minimum in the plasma density between the E and F regions, the so-called valley. Here a thin layer of a strongly-elevated electron temperature and airglow is predicted. Neutralizing electric currents carried by ionospheric electrons can become unstable in the low-density valley. As a result, developing plasma waves inhibit the currents. In the extreme case, the beam might be locked (a 'virtual cathode'). In addition to optical observations, these effects can also be observed by radio frequency methods. C1 Boston Coll, Inst Sci Res, Chestnut Hill, MA 02467 USA. NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA. RP Mishin, EV (reprint author), Boston Coll, Inst Sci Res, 402 St Clements Hall,140 Commonwealth Ave, Chestnut Hill, MA 02467 USA. EM evgenii.mishin@hanscom.af.mil; george.khazanov@nsstc.nasa.gov NR 28 TC 3 Z9 3 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 AUG 4 PY 2006 VL 33 IS 15 AR L15105 DI 10.1029/2006GL026220 PG 4 WC Geosciences, Multidisciplinary SC Geology GA 071JF UT WOS:000239596800003 ER PT J AU Kaufman, YJ Koren, I AF Kaufman, Yoram J. Koren, Ilan TI Smoke and pollution aerosol effect on cloud cover SO SCIENCE LA English DT Article ID OPTICAL-PROPERTIES; AIR-POLLUTION; CLIMATE; RAIN; ATMOSPHERE; AERONET; AMAZON; OCEAN; MODIS; SOOT AB Pollution and smoke aerosols can increase or decrease the cloud cover. This duality in the effects of aerosols forms one of the largest uncertainties in climate research. Using solar measurements from Aerosol Robotic Network sites around the globe, we show an increase in cloud cover with an increase in the aerosol column concentration and an inverse dependence on the aerosol absorption of sunlight. The emerging rule appears to be independent of geographical location or aerosol type, thus increasing our confidence in the understanding of these aerosol effects on the clouds and climate. Preliminary estimates suggest an increase of 5% in cloud cover. C1 Weizmann Inst Sci, Dept Environm Sci & Energy Res, IL-76100 Rehovot, Israel. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Koren, I (reprint author), Weizmann Inst Sci, Dept Environm Sci & Energy Res, IL-76100 Rehovot, Israel. EM ilan.koren@weizmann.ac.il RI Koren, Ilan/K-1417-2012 OI Koren, Ilan/0000-0001-6759-6265 NR 34 TC 150 Z9 156 U1 2 U2 28 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 AUG 4 PY 2006 VL 313 IS 5787 BP 655 EP 658 DI 10.1126/science.1126232 PG 4 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 072IQ UT WOS:000239667500039 PM 16840661 ER PT J AU Jin, JJ Semeniuk, K Manney, GL Jonsson, AI Beagley, SR McConnell, JC Dufour, G Nassar, R Boone, CD Walker, KA Bernath, PF Rinsland, CP AF Jin, J. J. Semeniuk, K. Manney, G. L. Jonsson, A. I. Beagley, S. R. McConnell, J. C. Dufour, G. Nassar, R. Boone, C. D. Walker, K. A. Bernath, P. F. Rinsland, C. P. TI Severe Arctic ozone loss in the winter 2004/2005: observations from ACE-FTS SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID POLAR VORTEX AIR; ART.; DENITRIFICATION AB The severe Arctic ozone reduction in the winter 2004/ 2005 is analyzed using ACE-FTS observations and four different analysis techniques: correlations between ozone and long-lived tracers ( adjusted to account for mixing), an artificial tracer correlation method, a profile-descent technique, and the empirical relationship between ozone loss and potential PSC volume. The average maximum ozone loss was about 2.1 ppmv at 475 K - 500 K ( similar to 18 km 20 km). Over 60% of the ozone between 425 K - 475 K ( similar to 16 km - 18 km) was destroyed. The average total column ozone loss was 119 DU, similar to 20 - 30 DU larger than the largest previously observed Arctic ozone loss in the winter 1999/ 2000. C1 York Univ, Dept Earth & Space Sci & Engn, N York, ON M3J 1P3, Canada. CALTECH, Jet Propuls Lab, Pasadena, CA 91109 USA. New Mexico Inst Min & Technol, Socorro, NM 87801 USA. Univ Waterloo, Dept Chem, Waterloo, ON N2L 3G1, Canada. NASA, Langley Res Ctr, Hampton, VA 23681 USA. RP Jin, JJ (reprint author), York Univ, Dept Earth & Space Sci & Engn, 4700 Keele St, N York, ON M3J 1P3, Canada. EM jianjun@yorku.ca RI Bernath, Peter/B-6567-2012; Jin, Jianjun/G-8357-2012; Jonsson, Andreas/B-3887-2013; OI Bernath, Peter/0000-0002-1255-396X; Jonsson, Andreas/0000-0003-0321-6213; Nassar, Ray/0000-0001-6282-1611 NR 26 TC 32 Z9 32 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 AUG 2 PY 2006 VL 33 IS 15 AR L15801 DI 10.1029/2006GL026752 PG 5 WC Geosciences, Multidisciplinary SC Geology GA 071JC UT WOS:000239596500006 ER PT J AU Kunhikrishnan, T Lawrence, MG von Kuhlmann, R Wenig, MO Asman, WAH Richter, A Burrows, JP AF Kunhikrishnan, T. Lawrence, Mark G. von Kuhlmann, Rolf Wenig, Mark O. Asman, Willem A. H. Richter, Andreas Burrows, John P. TI Regional NOx emission strength for the Indian subcontinent and the impact of emissions from India and neighboring countries on regional O-3 chemistry SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID MOZAIC AIRBORNE PROGRAM; IN-SERVICE AIRCRAFT; TROPOSPHERIC OZONE; AIR-POLLUTION; NONMETHANE HYDROCARBONS; SATELLITE-OBSERVATIONS; GLOBAL DISTRIBUTIONS; URBAN ATMOSPHERE; NORTH-AMERICA; ASIA AB [ 1] This study examines the regional NOx emission strength and influence of external emissions on O-3-related chemistry over the Indian subcontinent based on a three-dimensional chemistry transport model and space-based observations, following up on our earlier work on NOx chemistry over southern Asia. NOx mass and emissions from Global Ozone Monitoring Experiment ( GOME) and Model of Atmospheric Transport and Chemistry-Max Planck Institute for Chemistry Version ( MATCH-MPIC) over India are compared, and the uncertainties in the estimates are briefly discussed. This study also employs the concept of small-perturbation tendencies to compute the scaled sensitivities with modified NOx emissions for India and the neighboring continents. The sensitivities of NOx, O-3, OH, and reservoir species of NOx over India to NOx emission from India, Southeast Asia, Africa, China, and the Middle East are discussed with respect to the photochemistry and the regional meteorology. Our study suggests that the mean regional NOx emission strength for India is close to 2.5 Tg( N)/ yr with a seasonal maximum (similar to 3 Tg( N)/ yr) during April and minimum (similar to 1.6 Tg( N)/ yr) during winter. The changes in the O3 concentrations with respect to NOx and nonmethane hydrocarbon emissions from India show that southern India is relatively more sensitive to local emission. C1 Max Planck Inst Chem, Dept Atmospher Chem, D-55020 Mainz, Germany. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Univ Bremen, Dept Environm Phys & Remote Sensing, D-28359 Bremen, Germany. RP Kunhikrishnan, T (reprint author), NASA, Langley Res Ctr, Atmospher Sci Directorate, 100 NASA Rd, Hampton, VA 23681 USA. RI Richter, Andreas/C-4971-2008 OI Richter, Andreas/0000-0003-3339-212X NR 51 TC 24 Z9 24 U1 1 U2 10 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X EI 2169-8996 J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD AUG 2 PY 2006 VL 111 IS D15 AR D15301 DI 10.1029/2005JD006036 PG 16 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 071JJ UT WOS:000239597400001 ER PT J AU Uitz, J Claustre, H Morel, A Hooker, SB AF Uitz, Julia Claustre, Herve Morel, Andre Hooker, Stanford B. TI Vertical distribution of phytoplankton communities in open ocean: An assessment based on surface chlorophyll SO JOURNAL OF GEOPHYSICAL RESEARCH-OCEANS LA English DT Article ID ECOSYSTEM MODEL; EUPHOTIC ZONE; BIOOPTICAL PROPERTIES; NORTH-ATLANTIC; ROSS-SEA; VARIABILITY; PIGMENTS; WATERS; ALGORITHMS; PACIFIC AB The present study examines the potential of using the near-surface chlorophyll a concentration ([Chla](surf)), as it can be derived from ocean color observation, to infer the column-integrated phytoplankton biomass, its vertical distribution, and ultimately the community composition. Within this context, a large High-Performance Liquid Chromatography (HPLC) pigment database was analyzed. It includes 2419 vertical pigment profiles, sampled in case 1 waters with various trophic states (0.03-6 mg Chla m(-3)). The relationships between [Chla](surf) and the chlorophyll a vertical distribution, as previously derived by Morel and Berthon (1989), are fully confirmed. This agreement makes it possible to go further and to examine if similar relationships between [Chla](surf) and the phytoplankton assemblage composition along the vertical can be derived. Thanks to the detailed pigment composition, and use of specific pigment biomarkers, the contribution to the local chlorophyll a concentration of three phytoplankton groups can be assessed. With some cautions, these groups coincide with three size classes, i.e., microplankton, nanoplankton and picoplankton. Corroborating previous regional findings (e.g., large species dominate in eutrophic environments, whereas tiny phytoplankton prevail in oligotrophic zones), the present results lead to an empirical parameterization applicable to most oceanic waters. The predictive skill of this parameterization is satisfactorily tested on a separate data set. With such a tool, the vertical chlorophyll a profiles of each group can be inferred solely from the knowledge of [Chla](surf). By combining this tool with satellite ocean color data, it becomes possible to quantify on a global scale the phytoplankton biomass associated with each of the three algal assemblages. C1 CNRS, UMR 7093, Lab Oceanog Villefranche, F-06238 Villefranche Sur Mer, France. Univ Paris 06, F-06238 Villefranche Sur Mer, France. NASA, Goddard Space Flight Ctr, Lab Hydrospher Proc, Greenbelt, MD 20771 USA. RP Uitz, J (reprint author), CNRS, UMR 7093, Lab Oceanog Villefranche, BP 08, F-06238 Villefranche Sur Mer, France. EM uitz@obs-vlfr.fr RI Hooker, Stanford/E-2162-2012; CLAUSTRE, Herve/E-6877-2011 OI CLAUSTRE, Herve/0000-0001-6243-0258 NR 48 TC 233 Z9 245 U1 9 U2 69 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9275 EI 2169-9291 J9 J GEOPHYS RES-OCEANS JI J. Geophys. Res.-Oceans PD AUG 2 PY 2006 VL 111 IS C8 AR C08005 DI 10.1029/2005JC003207 PG 23 WC Oceanography SC Oceanography GA 071JN UT WOS:000239597900001 ER PT J AU Baudin, C Sayir, A Berger, MH AF Baudin, C. Sayir, A. Berger, M. H. TI Mechanical behaviour of directionally solidified alumina/aluminium titanate ceramics SO ACTA MATERIALIA LA English DT Article DE directional solidification; eutectic solidification; ceramic; fracture; flaw tolerance ID THERMAL-EXPANSION DATA; ALUMINUM TITANATE; EUTECTIC COMPOSITES; CREEP RESISTANCE; TEMPERATURE; MICROSTRUCTURE; STABILITY; STRENGTH; DESIGN AB Directionally solidified eutectic ceramics of the alumina-titania system have been developed. Compositions from the alumina-rich part of the phase diagram were included in the study. The challenge was to produce materials that combine strength and flaw tolerance. A eutectic with 44 mol% TiO2 and two off-eutectics consisting of 12 and 26 mol% TiO2 were chosen for the study. The specimens exhibited a highly oriented microstructure that was aligned with the growth axis. The material with eutectic composition consisted of Al6Ti2O13/Al2TiO5 lamellae arranged in rods separated by longitudinal cracks. The materials with off-eutectic compositions consisted of alumina dendrites separated by Al6Ti2O13 matrix. Three-point bending tests and fractographic analyses revealed the high strains before failure. The eutectic rods and the alumina dendrites ensured a load-bearing capability. Cracks were arrested by the longitudinal pre-existing cracks in the eutectic composition material and were deflected at the alumina/aluminium titanate interfaces in the off-eutectic samples. This crack-crack interaction and associated change in load transfer conditions produced non-linear load-displacement curves, high failure strains and non-planar fracture surfaces. (c) 2006 Acta Materialia Inc. Published by Elsevier Ltd. All rights reserved. C1 CSIC, Inst Ceram & Vidrio, Madrid 28049, Spain. NASA, GRC, CWRU, Cleveland, OH 44135 USA. Ecole Mines Paris, Ctr Mat, F-91003 Evry, France. RP Baudin, C (reprint author), CSIC, Inst Ceram & Vidrio, Kelsen 5, Madrid 28049, Spain. EM cbaudin@icv.csic.es RI Berger, Marie-Helene/B-9785-2013; OI Baudin, Carmen/0000-0002-9037-0931 NR 28 TC 21 Z9 24 U1 1 U2 18 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 1359-6454 EI 1873-2453 J9 ACTA MATER JI Acta Mater. PD AUG PY 2006 VL 54 IS 14 BP 3835 EP 3841 DI 10.1016/j.actamat.2006.04.015 PG 7 WC Materials Science, Multidisciplinary; Metallurgy & Metallurgical Engineering SC Materials Science; Metallurgy & Metallurgical Engineering GA 079JH UT WOS:000240171400020 ER PT J AU Przekop, A Rizzi, SA AF Przekop, Adam Rizzi, Stephen A. TI Nonlinear reduced order random response analysis of structures with shallow curvature SO AIAA JOURNAL LA English DT Article; Proceedings Paper CT AIAA/ASME/ASCE/AHS/ASC 46th Structures, Structural Dynamics and Materials Conference/1st AIAA Multidisciplinary Design Optimization Specialist Conference CY APR 18-21, 2005 CL Austin, TX SP AIAA, ASME, ASCE, AHS, ASC ID VIBRATION; SHELLS AB The goal of this investigation is to further develop nonlinear modal numerical simulation methods for application to geometrically nonlinear response of structures with shallow curvature under random loadings. For reduced order analysis, the modal basis selection must be capable of reflecting the coupling in both the linear and nonlinear stiffness. For the symmetric shallow arch under consideration, four categories of modal basis functions are defined. Modal bases having symmetric transverse displacements and modal bases having anti-symmetric transverse displacements may each be either transverse dominated or in-plane dominated. The response of an aluminum arch under a uniformly distributed transverse random loading is investigated. Results from nonlinear modal simulations made using various modal bases are compared with those obtained from a numerical simulation in physical degrees-of-freedom. While inclusion of transverse dominated modes having a symmetric transverse displacement is important for all response regimes, it is found that the in-plane dominated modes having a symmetric transverse displacement become increasingly important in the nonlinear response regime. In the autoparametric response regime, the inclusion of both transverse and in-plane dominated modes, each with an anti-symmetric transverse displacement distribution, is found to be critical. C1 Natl Inst Aerosp, Hampton, VA 23666 USA. NASA, Langley Res Ctr, Hampton, VA 23681 USA. RP Przekop, A (reprint author), Natl Inst Aerosp, Hampton, VA 23666 USA. NR 20 TC 20 Z9 21 U1 0 U2 4 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 AUG PY 2006 VL 44 IS 8 BP 1767 EP 1778 DI 10.2514/1.18868 PG 12 WC Engineering, Aerospace SC Engineering GA 070NJ UT WOS:000239529100007 ER PT J AU Dudek, JC AF Dudek, Julianne C. TI Empirical model for vane-type vortex generators in a Navier-Stokes code 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 AB An empirical model which simulates the effects of vane-type vortex generators in ducts was incorporated into. the Wind-US Navier-Stokes computational fluid dynamics code. The model enables the effects of the vortex generators to be simulated without defining the details of the geometry within the grid, and makes it practical for researchers to evaluate multiple combinations of vortex generator arrangements. The model determines the strength of each vortex based on the generator geometry and the local flow conditions. Validation results are presented for three duct geometries containing vortex generators: a straight pipe, a transitioning S-duct diffuser, and a circular S-duct diffuser. The computations made using the vortex generator model are compared with computations made using gridded vanes as well as with experimental data. C1 NASA, Glenn Res Ctr, Brookpark, OH 44135 USA. RP Dudek, JC (reprint author), NASA, Glenn Res Ctr, Brookpark, OH 44135 USA. NR 18 TC 7 Z9 7 U1 1 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 AUG PY 2006 VL 44 IS 8 BP 1779 EP 1789 DI 10.2514/1.20141 PG 11 WC Engineering, Aerospace SC Engineering GA 070NJ UT WOS:000239529100008 ER PT J AU Cabell, RH Kegerise, MA Cox, DE Gibbs, GP AF Cabell, Randolph H. Kegerise, Michael A. Cox, David E. Gibbs, Gary P. TI Experimental feedback control of flow-induced cavity tones SO AIAA JOURNAL LA English DT Article; Proceedings Paper CT AIAA/CEAS 8th Aeroacoustics Conference CY JUN 17-19, 2002 CL Breckenridge, CO SP Amer Inst Aeronaut & Astronaut, CEAS AB Discrete-time, linear quadratic methods were used to design feedback controllers for reducing tones generated by flow over a cavity. The dynamics of a sypthetic-jet actuator mounted at the leading edge of the cavity as observed by two microphones in the cavity were modeled over a broad frequency range using state space models computed from experimental data. Variations in closed loop performance as a function of model order, control order, control bandwidth, and state estimator design were studied using a cavity in the Probe Calibration Tunnel at NASA Langley Research Center. The controller successfully reduced the levels of multiple cavity tones at the tested flow speeds of Mach 0.275, 0.35, and 0.45. In some cases, the closed loop results were limited by excitation of sidebands of the cavity tones, or the creation of new tones at frequencies away from the cavity tones. The models were not able to account for nonlinear dynamics, such as interactions between tones at different frequencies. Nonetheless, the results validate the combination of optimal control and experimentally generated state space models for the cavity tone problem. C1 NASA, Langley Res Ctr, Hampton, VA 23681 USA. RP Cabell, RH (reprint author), NASA, Langley Res Ctr, Hampton, VA 23681 USA. EM randolph.h.cabell@nasa.gov; michael.a.kegerise@nasa.gov; david.e.cox@nasa.gov; gary.p.gibbs@nasa.gov NR 28 TC 9 Z9 9 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 AUG PY 2006 VL 44 IS 8 BP 1807 EP 1815 DI 10.2514/1.19608 PG 9 WC Engineering, Aerospace SC Engineering GA 070NJ UT WOS:000239529100011 ER PT J AU Chowdhary, J Cairns, B Travis, LD AF Chowdhary, Jacek Cairns, Brian Travis, Larry D. TI Contribution of water-leaving radiances to multiangle, multispectral polarimetric observations over the open ocean: bio-optical model results for case 1 waters SO APPLIED OPTICS LA English DT Review ID MOLECULAR-SCATTERING CONTRIBUTION; RESEARCH SCANNING POLARIMETER; PARTICLE-SIZE DISTRIBUTION; DISSOLVED ORGANIC-MATTER; LIGHT-SCATTERING; POLARIZED-LIGHT; DIFFUSE-REFLECTANCE; OPTICAL-PROPERTIES; REFRACTIVE-INDEX; PLANETARY-ATMOSPHERES AB Multiangle, multispectral photopolarimetry of atmosphere-ocean systems provides the fullest set of remote sensing information possible on the scattering properties of aerosols and on the color of the ocean. Recent studies have shown that inverting such data allows for the potential of separating the retrieval of aerosol properties from ocean color monitoring in the visible part of the spectrum. However, the data in these studies were limited to those principal plane observations where the polarization of water-leaving radiances could be ignored. Examining similar potentials for off-principal plane observations requires the ability to assess realistic variations in both the reflectance for and bidirectionality of polarized water-leaving radiances for such viewing geometries. We provide hydrosol models for use in underwater light scattering computations to study such variations. The model consists of two components whose refractive indices resemble those of detritus-minerallike and planktonlike particles, whose size distributions are constrained by underwater light linear polarization signatures, and whose mixing ratios change as a function of particulate backscattering efficiency. Multiple scattering computations show that these models are capable of reproducing realistic underwater light albedos for wavelengths ranging from 400 to 600 nm, and for chlorophyll a concentrations ranging from 0.03 to 3.0 mg/m(3). Numerical results for spaceborne observations of the reflectance for total and polarized water-leaving radiances are provided as a function of polar angles, and the change in these reflectances with wavelength, chlorophyll a concentration, and hydrosol model are discussed in detail for case 1 (open ocean) waters. (C) 2006 Optical Society of America. C1 Columbia Univ, Dept Appl Phys & Appl Math, New York, NY 10025 USA. NASA, Goddard Inst Space Studies, New York, NY 10025 USA. RP Chowdhary, J (reprint author), Columbia Univ, Dept Appl Phys & Appl Math, 2880 Broadway, New York, NY 10025 USA. EM jchowdhary@giss.nasa.gov OI Cairns, Brian/0000-0002-1980-1022 NR 102 TC 54 Z9 55 U1 0 U2 5 PU OPTICAL SOC AMER PI WASHINGTON PA 2010 MASSACHUSETTS AVE NW, WASHINGTON, DC 20036 USA SN 1559-128X EI 2155-3165 J9 APPL OPTICS JI Appl. Optics PD AUG 1 PY 2006 VL 45 IS 22 BP 5542 EP 5567 DI 10.1364/AO.45.005542 PG 26 WC Optics SC Optics GA 068YN UT WOS:000239411400010 PM 16855652 ER PT J AU Konishi, T Ito, A Kudo, Y Narurni, A Saito, K Baker, J Struk, PM AF Konishi, Tadashi Ito, Akihiko Kudo, Yuji Narurni, Akira Saito, Kozo Baker, John Struk, Peter M. TI Simultaneous measurement of temperature and chemical species concentrations with a holographic interferometer and infrared absorption SO APPLIED OPTICS LA English DT Article ID FUEL-CONCENTRATION; FLAME SPREAD; COLLAPSE; LIQUIDS; TOWERS AB What is believed to be a new technique that allows for the simultaneous measurement of 2D temperature and chemical species concentration profiles with high spatial resolution and fast time response was developed and tested successfully by measuring a thin layer of fuel vapor created over a volatile fuel surface. Normal propanol was placed in an open-top rectangular container, and n-propanol fuel vapor was formed over the propanol surface in a quiescent laboratory environment. An IR beam with a wavelength of 8-13 mu m emitted from a heated plate and a He-Ne laser beam with a wavelength of 632 nm were combined and passed through the n-propanol vapor layer, and both beams were absorbed by the vapor layer. The absorption of the IR beam was recorded by an IR camera, and the He-Ne laser was used to form a holographic interferogram. Two-dimensional temperature and propanol vapor concentration profiles were, respectively, determined by the IR absorption and the fringe pattern associated with the holographic interferogram. This new measurement technique is a significant improvement over the dual wavelength holographic interferometry that has been used previously to measure temperature and fuel concentration, and it is ready for application under different types of fire and flame conditions. (C) 2006 Optical Society of America. C1 Oita Natl Coll Technol, Dept Mech Engn, Oita 8700152, Japan. Hirosaki Univ, Dept Intelligent Machine & Syst Engn, Hirosaki, Aomori 0368561, Japan. Kanagawa Inst Technol, Dept Mech Engn, Atsugi, Kanagawa, Japan. Univ Kentucky, Dept Mech Engn, Lexington, KY 40506 USA. Univ Alabama, Dept Mech Engn, Tuscaloosa, AL 35487 USA. NASA, Glenn Res Ctr, Combust & React Syst Branch, Cleveland, OH 44135 USA. RP Konishi, T (reprint author), Oita Natl Coll Technol, Dept Mech Engn, 1666 Maki, Oita 8700152, Japan. EM saito@engr.uky.edu NR 20 TC 5 Z9 5 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 AUG 1 PY 2006 VL 45 IS 22 BP 5725 EP 5732 DI 10.1364/AO.45.005725 PG 8 WC Optics SC Optics GA 068YN UT WOS:000239411400030 PM 16855672 ER PT J AU Sharma, SK Misra, AK Lucey, PG Angel, SM Mckay, CP AF Sharma, S. K. Misra, A. K. Lucey, P. G. Angel, S. M. Mckay, C. P. TI Remote pulsed Raman spectroscopy of inorganic and organic materials to a radial distance of 100 meters SO APPLIED SPECTROSCOPY LA English DT Article DE Raman spectroscopy; gated remote Raman; inorganic and organic compounds; planetary Raman; portable remote Raman system; daytime Raman spectroscopy ID VIBRATIONAL SPECTRA; PLANETARY SURFACES; CRYSTALLINE STATE; SINGLE-CRYSTALS; FILTER; SYSTEM AB A portable pulsed remote Raman spectroscopy system has been fabricated and tested to 100 m radial distance. The remote Raman system is based on a directly coupled f/2.2 spectrograph with a small (125 mm diameter) telescope and a frequency-doubled Nd:YAG pulsed laser (20 Hz, 532 nm, 25 mJ/pulse) used as the excitation source in a co-axial geometry. The performance of the Raman system is demonstrated by measuring the gated Raman spectra of calcite, sodium phosphate, acetone, and naphthalene. Raman spectra of these materials were recorded with the 532 run pulsed laser excitation and accumulating the spectra with 600 laser shots (30 s integration time) at 100 m with good signal-to-background ratio. The remote pulsed Raman system can be used for remotely identifying both inorganic and organic materials during daytime or nighttime. The system will be useful for terrestrial applications such as monitoring environmental pollution and for detecting minerals and organic materials such as polycyclic aromatic hydrocarbons (PAHs) on planetary surfaces such as Mars. C1 Univ Hawaii, Hawaii Inst Geophys & Planetol, SOEST, Honolulu, HI 96822 USA. Univ S Carolina, Dept Chem & Biochem, Columbia, SC 29208 USA. NASA, Ames Res Ctr, Div Space Sci, Moffett Field, CA 94035 USA. RP Sharma, SK (reprint author), Univ Hawaii, Hawaii Inst Geophys & Planetol, SOEST, 1680 EW Rd,Post 602, Honolulu, HI 96822 USA. EM sksharma@soest.hawaii.edu OI Angel, Stanley/0000-0002-0328-0568 NR 20 TC 45 Z9 46 U1 0 U2 11 PU SOC APPLIED SPECTROSCOPY PI FREDERICK PA 201B BROADWAY ST, FREDERICK, MD 21701 USA SN 0003-7028 J9 APPL SPECTROSC JI Appl. Spectrosc. PD AUG PY 2006 VL 60 IS 8 BP 871 EP 876 DI 10.1366/000370206778062110 PG 6 WC Instruments & Instrumentation; Spectroscopy SC Instruments & Instrumentation; Spectroscopy GA 075VF UT WOS:000239912900006 PM 16925922 ER PT J AU Vasudev, R AF Vasudev, R. TI Wavelength modulated cavity enhanced absorption spectroscopy of water in the 1.37 mu m region SO APPLIED SPECTROSCOPY LA English DT Article DE water; isotopomers; planetary; mars; diode laser; near-infrared spectroscopy ID RING-DOWN SPECTROSCOPY; TRACE GAS-DETECTION; LASER; ATMOSPHERE; METHANE; MARS AB We describe the performance of a high-sensitivity wavelength modulated cavity enhanced infrared tunable diode laser absorption spectrometer for the detection of water vapor in the 1.37 mu m region. The spectrometer can measure a fractional absorption of similar to 10(-5) for an absorption path length of a few kilometers. The instrument's sensitivity is more than sufficient to detect water isotopomers; ((H2O)-O-16, (H2O)-O-18, HDO) at Martian atmospheric concentrations. The instrument is amenable to miniaturization, so a future compact, multiple-species version of the spectrometer will be highly suitable for in situ planetary exploration. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Vasudev, R (reprint author), CALTECH, Jet Prop Lab, MS 183-401,4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM rvasudev@jpl.nasa.gov NR 31 TC 8 Z9 8 U1 1 U2 5 PU SOC APPLIED SPECTROSCOPY PI FREDERICK PA 201B BROADWAY ST, FREDERICK, MD 21701 USA SN 0003-7028 J9 APPL SPECTROSC JI Appl. Spectrosc. PD AUG PY 2006 VL 60 IS 8 BP 926 EP 930 DI 10.1366/000370206778062075 PG 5 WC Instruments & Instrumentation; Spectroscopy SC Instruments & Instrumentation; Spectroscopy GA 075VF UT WOS:000239912900014 PM 16925930 ER PT J AU Conley, CA Ishkhanova, G Mckay, CP Cullings, K AF Conley, Catharine A. Ishkhanova, Galina McKay, Christopher P. Cullings, Ken TI A preliminary survey of non-lichenized fungi cultured from the hyperarid Atacama Desert of Chile SO ASTROBIOLOGY LA English DT Article DE 16S rRNA; Caenorhabditis elegans maintenance medium; Ascomycota; Ustilago ID COMMUNITY; LIFE AB The Atacama Desert is one of the driest environments on Earth, and has been so for over 200,000 years. Previous reports have suggested that surprisingly low numbers of culturable bacteria, counted as biomass or species diversity, are present in Atacama sands collected from the most hyperarid regions. In previous studies, the presence of eukaryotic organisms was not discussed. In this report, we describe a method of direct plating onto rich media that resulted in culturing a range of fungi from Atacama samples. All fungi identified in this preliminary survey are spore-forming saprobes that are readily dispersed by wind, a likely mechanism that accounts for their presence in the central Atacama Desert. C1 NASA, Planetary Sci Div, Sci Miss Directorate, Washington, DC 20546 USA. NASA, Ames Res Ctr, Space Lifesci Res Branch, Moffett Field, CA 94035 USA. NASA, Ames Res Ctr, Div Space Sci, Moffett Field, CA 94035 USA. RP Conley, CA (reprint author), NASA, Planetary Sci Div, Sci Miss Directorate, Washington, DC 20546 USA. EM cassie.conley@nasa.gov NR 13 TC 22 Z9 22 U1 3 U2 13 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 AUG PY 2006 VL 6 IS 4 BP 521 EP 526 DI 10.1089/ast.2006.6.521 PG 6 WC Astronomy & Astrophysics; Biology; Geosciences, Multidisciplinary SC Astronomy & Astrophysics; Life Sciences & Biomedicine - Other Topics; Geology GA 077ZP UT WOS:000240070800001 PM 16916279 ER PT J AU Fallacaro, A Calvin, WM AF Fallacaro, Alicia Calvin, Wendy M. TI Spectral properties of Lake Superior banded iron formation: Application to martian hematite deposits SO ASTROBIOLOGY LA English DT Article DE banded iron formation; iron oxides; Mars; spectroscopy; analog ID X-RAY SPECTROMETER; MERIDIANI-PLANUM; EMISSION-SPECTROSCOPY; MARS PATHFINDER; BURNS FORMATION; MINERALOGY; ROCKS; SOILS; WATER; PHYLLOSILICATES AB Several locations have been identified on Mars that expose bulk, coarsely crystalline gray hematite. These deposits have been interpreted as being sedimentary and formed in aqueous environments. Lake Superior Type (LST) banded iron formation (BIF) was investigated as a spectral and possible process analog to these deposits. In northern Michigan, LST BIF formed in a sedimentary, continental shelf or shallow basin environment under stable tectonic conditions, and the oxide facies contains gray, crystalline hematite. These deposits are Proterozoic in age and contain microfossils associated with the early diversification of life on Earth. Samples of the hematite-bearing oxide facies, as well as the carbonate facies, were collected and analyzed for their spectral and geochemical characteristics. Sample spectra were measured in the visible, near-infrared, and thermal infrared for comparison with remote and in situ spectra obtained at Mars. Thin section analysis, as well as X-ray diffraction and scaning electron microscopy measurements, were performed to determine detailed geochemistry. There is no evidence for BIF at Opportunity's Meridiani landing site, and the results of this work will provide useful data for determining whether BIFs exist elsewhere on Mars and are, thus, relevant to current and future Mars exploration missions. C1 Univ Nevada, Reno, NV 89557 USA. RP Fallacaro, A (reprint author), CALTECH, Jet Prop Lab, MS 264-422,4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM Alica.F.Vaughan@jpl.nasa.gov NR 49 TC 1 Z9 1 U1 1 U2 7 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 AUG PY 2006 VL 6 IS 4 BP 563 EP 580 DI 10.1089/ast.2006.6.563 PG 18 WC Astronomy & Astrophysics; Biology; Geosciences, Multidisciplinary SC Astronomy & Astrophysics; Life Sciences & Biomedicine - Other Topics; Geology GA 077ZP UT WOS:000240070800005 PM 16916283 ER PT J AU Quinn, R Zent, AP Mckay, CP AF Quinn, Richard Zent, Aaron P. McKay, Christopher P. TI The photochemical stability of carbonates on Mars SO ASTROBIOLOGY LA English DT Article DE Mars, surface; photochemistry; carbonates ID DIOXIDE CLOUDS; CLIMATE; CO2; PHOTODISSOCIATION; EVOLUTION; MODEL AB Carbonates, predominately MgCO3, have been spectroscopically identified at a level of 2-5% in martian dust. However, in spite of this observation, and a large number of climate studies that suggest 1 to several bars of CO2 should be sequestered in carbonate rocks, no outcrop-scale exposures of carbonate have been detected anywhere on Mars to date. To address one hypothesis for this long-standing puzzle, the effect of ultraviolet (UV) light on the stability of calcium carbonate in a simulated martian atmosphere was experimentally investigated. Using C-13-labeled calcite, we found no experimental evidence of the UV photodecomposition of calcium carbonate in a simulated martian atmosphere. Extrapolating the lower limit of detection of our experimental system to an upper limit of carbonate decomposition on Mars yields a quantum efficiency of 3.5 x 10(-8) molecules/photon over the wavelength interval of 190-390 nm and a maximum UV photodecomposition rate of 1.2 x 10(-13) kg m(-2) s(-1) from a calcite surface. The maximum loss of bulk calcite due to this process would be 2.5 nm year(-1) (Mars year). However, calcite is expected to be thermodynamically stable on the surface of Mars, and potential UV photodecomposition reaction mechanisms indicate that, though calcium carbonate may decompose under vacuum, it would be stable in a CO2 atmosphere. Given the expected stability of carbonate on Mars and our inability to detect carbonate decomposition, we conclude that it is unlikely that the apparent absence of extensive carbonate deposits on the martian surface is due to UV photodecomposition in the current environment. C1 NASA, Ames Res Ctr, SETI Inst, Moffett Field, CA 94039 USA. RP Quinn, R (reprint author), NASA, Ames Res Ctr, SETI Inst, Mail Stop 239-12, Moffett Field, CA 94039 USA. EM rquinn@mail.arc.nasa.gov NR 27 TC 8 Z9 9 U1 1 U2 10 PU MARY ANN LIEBERT INC PI NEW ROCHELLE PA 140 HUGUENOT STREET, 3RD FL, NEW ROCHELLE, NY 10801 USA SN 1531-1074 J9 ASTROBIOLOGY JI Astrobiology PD AUG PY 2006 VL 6 IS 4 BP 581 EP 591 DI 10.1089/ast.2006.6.581 PG 11 WC Astronomy & Astrophysics; Biology; Geosciences, Multidisciplinary SC Astronomy & Astrophysics; Life Sciences & Biomedicine - Other Topics; Geology GA 077ZP UT WOS:000240070800006 PM 16916284 ER PT J AU Das, V Crenshaw, DM Kraemer, SB Deo, RP AF Das, V. Crenshaw, D. M. Kraemer, S. B. Deo, R. P. TI Kinematics of the narrow-line region in the Seyfert 2 galaxy NGC 1068: Dynamical effects of the radio jet SO ASTRONOMICAL JOURNAL LA English DT Article DE galaxies : individual (NGC 1068); galaxies : kinematics and dynamics; galaxies : Seyfert; ultraviolet : galaxies ID LONG-SLIT SPECTROSCOPY; NGC 1068; RESOLVED SPECTROSCOPY; PHYSICAL CONDITIONS; EMISSION-LINES; CENTRAL ENGINE; 3C 273; SPECTROPOLARIMETRY; NGC-4151; OUTFLOW AB We present a study of high-resolution long-slit spectra of the narrow-line region (NLR) in NGC 1068 obtained with the Space Telescope Imaging Spectrograph aboard the Hubble Space Telescope (HST). The spectra were retrieved from the Multimission Archive at the Space Telescope Science Institute obtained from two visits and seven orbits of HST time. We also obtained MERLIN radio maps of the center of NGC 1068 to examine the dependence of the NLR cloud velocities on the radio structure. The radial velocities and velocity dispersions of the bright NLR clouds appear to be unaffected by the radio knots, indicating that the radio jet is not the principal driving force on the outflowing NLR clouds. However, the velocities of the fainter NLR clouds are split near knots in the jet, indicating a possible interaction. Biconical outflow models were generated to match the data and for comparison to previous models done with lower dispersion observations. The general trend is an increase in radial velocity roughly proportional to distance from the nucleus followed by a linear decrease after roughly 100 pc similar to that seen in other Seyfert galaxies, indicating common acceleration and deceleration mechanisms. C1 Georgia State Univ, Dept Phys & Astron, Atlanta, GA 30303 USA. Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA. NASA Goddard Space Flight Ctr, Lab Astron & Solar Phys, Greenbelt, MD 20771 USA. RP Das, V (reprint author), Georgia State Univ, Dept Phys & Astron, 1 Park Pl South SE,Suite 700, Atlanta, GA 30303 USA. EM das@chara.gsu.edu; crenshaw@chara.gsu.edu; stiskraemer@yancey.gsfc.nasa.gov; deo@chara.gsu.edu NR 55 TC 61 Z9 61 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-6256 J9 ASTRON J JI Astron. J. PD AUG PY 2006 VL 132 IS 2 BP 620 EP 632 DI 10.1086/504899 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 072WA UT WOS:000239702500015 ER PT J AU Spitale, JN Jacobson, RA Porco, CC Owen, WM AF Spitale, J. N. Jacobson, R. A. Porco, C. C. Owen, W. M., Jr. TI The orbits of Saturn's small satellites derived from combined historic and Cassini imaging observations SO ASTRONOMICAL JOURNAL LA English DT Article DE planets : rings; planets and satellites : individual (Atlas, Daphnis, Epimetheus, Janus, Methone, Pallene, Pan, Pandora, Polydeuces, Prometheus) ID ADDITIONAL SMALL SATELLITES; RING-PLANE CROSSINGS; F-RING; ENCKE GAP; PROMETHEUS; PANDORA; MASSES; OCCULTATION; EXISTENCE; MOONLET AB We report on the orbits of the small, inner Saturnian satellites, either recovered or newly discovered in recent Cassini imaging observations. The orbits presented here reflect improvements over our previously published values in that the time base of Cassini observations has been extended, and numerical orbital integrations have been performed in those cases in which simple precessing elliptical, inclined orbit solutions were found to be inadequate. Using combined Cassini and Voyager observations, we obtain an eccentricity for Pan 7 times smaller than previously reported because of the predominance of higher quality Cassini data in the fit. The orbit of the small satellite (S/2005 S1 [Daphnis]) discovered by Cassini in the Keeler gap in the outer A ring appears to be circular and coplanar; no external perturbations are apparent. Refined orbits of Atlas, Prometheus, Pandora, Janus, and Epimetheus are based on Cassini, Voyager, Hubble Space Telescope, and Earth-based data and a numerical integration perturbed by all the massive satellites and each other. Atlas is significantly perturbed by Prometheus, and to a lesser extent by Pandora, through high-wavenumber mean-motion resonances. Orbital integrations involving Atlas yield a mass of GM(Atlas) (0.44 +/- 0.04) x 10(-3) km(3) s(-2), 3 times larger than reported previously ( GM is the product of the Newtonian constant of gravitation G and the satellite mass M). Orbital integrations show that Methone is perturbed by Mimas, Pallene is perturbed by Enceladus, and Polydeuces librates around Dione's L5 point with a period of about 791 days. We report on the nature and orbits of bodies sighted in the F ring, two of which may have persisted for a year or more. C1 CICLOPS, Space Sci Inst, Boulder, CO 80301 USA. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Spitale, JN (reprint author), CICLOPS, Space Sci Inst, 4750 Walnut St,Suite 205, Boulder, CO 80301 USA. EM spitale@lpl.arizona.edu NR 41 TC 43 Z9 43 U1 0 U2 2 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-6256 J9 ASTRON J JI Astron. J. PD AUG PY 2006 VL 132 IS 2 BP 692 EP 710 DI 10.1086/505206 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 072WA UT WOS:000239702500020 ER PT J AU Jacobson, RA Spitale, J Porco, CC Owen, WM AF Jacobson, R. A. Spitale, J. Porco, C. C. Owen, W. M., Jr. TI The GM values of Mimas and Tethys and the libration of methone SO ASTRONOMICAL JOURNAL LA English DT Article DE planets and satellites : individual (Mimas, Tethys) ID MAJOR SATURNIAN SATELLITES; CASSINI IMAGING SCIENCE; ORBITS; MASSES AB We have determined the GM of the Saturnian satellite Mimas from an analysis of its resonance with Tethys and with the newly discovered satellite Methone ( GM is the product of the Newtonian constant of gravitation G and the satellite's mass M). Observations of the latter permit a factor of 5 improvement in our knowledge of Mimas's GM; its value is 2.504 +/- 0.002 km(3) s(-2). Tethys's GM was originally found from the Mimas-Tethys resonance. We, however, estimate it using observations of its two Lagrangian satellites, Calypso and Telesto; its value is 41.200 +/- 0.007 km(3) s(-2). C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. CICLOPS, Space Sci Inst, Boulder, CO 80301 USA. RP Jacobson, RA (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM robert.jacobson@jpl.nasa.gov NR 15 TC 7 Z9 7 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-6256 J9 ASTRON J JI Astron. J. PD AUG PY 2006 VL 132 IS 2 BP 711 EP 713 DI 10.1086/505209 PG 3 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 072WA UT WOS:000239702500021 ER PT J AU Cool, RJ Kochanek, CS Eisenstein, DJ Stern, D Brand, K Brown, MJI Dey, A Eisenhardt, PR Fan, XH Gonzalez, AH Green, RF Jannuzi, BT McKenzie, EH Rieke, GH Rieke, M Soifer, BT Spinrad, H Elston, RJ AF Cool, Richard J. Kochanek, Christopher S. Eisenstein, Daniel J. Stern, Daniel Brand, Kate Brown, Michael J. I. Dey, Arjun Eisenhardt, Peter R. Fan, Xiaohui Gonzalez, Anthony H. Green, Richard F. Jannuzi, Buell T. McKenzie, Eric H. Rieke, George H. Rieke, Marcia Soifer, Baruch T. Spinrad, Hyron Elston, Richard J. TI The discovery of three new z > 5 quasars in the AGN and Galaxy Evolution Survey SO ASTRONOMICAL JOURNAL LA English DT Article DE quasars : emission lines; quasars : general ID DIGITAL-SKY-SURVEY; SURVEY COMMISSIONING DATA; SPITZER-SPACE-TELESCOPE; FALL EQUATORIAL STRIPE; FIBER-FED SPECTROGRAPH; QSO REDSHIFT SURVEY; ARRAY CAMERA IRAC; LUMINOSITY FUNCTION; ADDITIONAL QUASARS; X-RAY AB We present the discovery of three z > 5 quasars in the AGN and Galaxy Evolution Survey spectroscopic observations of the NOAO Deep Wide-Field Survey (NDWFS) Bootes Field. These quasars were selected as part of a larger Spitzer mid-infrared quasar sample, with no selection based on optical colors. The highest redshift object, NDWFS J142516.3+325409, at z 5: 85, is the lowest luminosity z = 5.8 quasar currently known. We compare mid-infrared techniques for identifying z > 5 quasars to more traditional optical techniques and show that mid-infrared colors allow for the selection of high-redshift quasars even at redshifts at which quasars lie near the optical stellar locus and at z > 7, where optical selection is impossible. Using the superb multiwavelength coverage available in the NDWFS Bootes field, we construct the spectral energy distributions (SEDs) of high-redshift quasars from observed BW band to 24 mu m (rest-frame 600 angstrom-3.7 mu m). We show that the three high-redshift quasars have quite similar SEDs, and the rest-frame composite SED of low-redshift quasars from the literature shows little evolution compared to our high-redshift objects. We compare the number of z > 5 quasars we have discovered to the expected number from published quasar luminosity functions. While analyses of the quasar luminosity function are tenuous based on only three objects, we find that a relatively steep luminosity function with Psi alpha L-3.2 provides the best agreement with the number of high-redshift quasars discovered in our survey. C1 Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. Ohio State Univ, Dept Astron, Columbus, OH 43210 USA. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. Natl Opt Astron Observ, Tucson, AZ 85726 USA. Princeton Univ Observ, Princeton, NJ 08544 USA. Univ Florida, Dept Astron, Gainesville, FL 32611 USA. Univ Arizona, Large Binocular Telescope Observ, Tucson, AZ 85721 USA. CALTECH, Div Phys Math & Astron, Pasadena, CA 91125 USA. CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA. Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. RP Cool, RJ (reprint author), Univ Arizona, Steward Observ, 933 N Cherry Ave, Tucson, AZ 85721 USA. EM rcool@as.arizona.edu RI Brown, Michael/B-1181-2015 OI Brown, Michael/0000-0002-1207-9137 NR 55 TC 45 Z9 45 U1 0 U2 2 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-6256 J9 ASTRON J JI Astron. J. PD AUG PY 2006 VL 132 IS 2 BP 823 EP 830 DI 10.1086/505535 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 072WA UT WOS:000239702500030 ER PT J AU Teplitz, HI Siana, B Brown, TM Chary, R Colbert, JW Conselice, CJ de Mello, DF Dickinson, M Ferguson, HC Gardner, JP Menanteau, F AF Teplitz, H. I. Siana, B. Brown, T. M. Chary, R. Colbert, J. W. Conselice, C. J. de Mello, D. F. Dickinson, M. Ferguson, H. C. Gardner, Jonathan P. Menanteau, F. TI Far-ultraviolet imaging of the Hubble Deep Field-North: Star formation in normal galaxies at z < 1 SO ASTRONOMICAL JOURNAL LA English DT Article DE cosmology : observations; galaxies : evolution; ultraviolet : galaxies ID SPECTRAL ENERGY-DISTRIBUTIONS; SPACE-TELESCOPE; LUMINOSITY DENSITY; FORMATION HISTORY; STARBURST GALAXIES; DUST ATTENUATION; FORMING GALAXIES; REDSHIFT SURVEY; STELLAR POPULATIONS; ELLIPTIC GALAXIES AB We present far-ultraviolet (FUV) imaging of the Hubble Deep Field-North (HDF-N) taken with the Solar Blind Channel of the Advanced Camera for Surveys (ACS SBC) and the FUV MAMA detector of the Space Telescope Imaging Spectrograph onboard the Hubble Space Telescope. The full WFPC2 deep field has been observed at 1600 angstrom. We detect 134 galaxies and one star down to a limit of FUVAB similar to 29. All sources have counterparts in the WFPC2 image. Redshifts (spectroscopic or photometric) for the detected sources are in the range 0 < z < 1. We find that the FUV galaxy number counts are higher than those reported by GALEX, which we attribute at least in part to cosmic variance in the small HDF-N field of view. Six of the 13 Chandra sources at z < 0.85 in the HDF-N are detected in the FUV, and those are consistent with starbursts rather than active galactic nuclei. Cross-correlating with Spitzer sources in the field, we find that the FUV detections show general agreement with the expected L-IR/L-UV versus beta relationship. We infer star formation rates (SFRs), corrected for extinction using the UV slope, and find a median value of 0.3 M-circle dot yr(-1) for FUV-detected galaxies, with 75% of detected sources having SFR < 1 M-circle dot yr(-1). Examining the morphological distribution of sources, we find that about half of all FUV-detected sources are identified as spiral galaxies. Half of morphologically selected spheroid galaxies at z < 0: 85 are detected in the FUV, suggesting that such sources have had significant ongoing star formation in the epoch since z similar to 1. C1 CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA. Space Telescope Sci Inst, Baltimore, MD 21218 USA. Univ Nottingham, Nottingham NG7 2RD, England. NASA, Goddard Space Flight Ctr, Observ Cosmol, Explorat Universe Div, Greenbelt, MD 20771 USA. Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA. Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. Natl Opt Astron Observ, Tucson, AZ 85719 USA. RP Teplitz, HI (reprint author), CALTECH, Spitzer Sci Ctr, MS 220-6, Pasadena, CA 91125 USA. EM hit@ipac.caltech.edu RI Conselice, Christopher/B-4348-2013; OI Brown, Thomas/0000-0002-1793-9968; Conselice, Christopher/0000-0003-1949-7638 NR 68 TC 24 Z9 24 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-6256 J9 ASTRON J JI Astron. J. PD AUG PY 2006 VL 132 IS 2 BP 853 EP 865 DI 10.1086/505685 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 072WA UT WOS:000239702500033 ER PT J AU Barmby, P Kuntz, KD Huchra, JP Brodie, JP AF Barmby, P. Kuntz, K. D. Huchra, J. P. Brodie, J. P. TI Hubble Space Telescope observations of star clusters in M101 SO ASTRONOMICAL JOURNAL LA English DT Article DE galaxies : individual ( M101); galaxies : spiral; galaxies : star clusters ID SCALE KEY PROJECT; GLOBULAR-CLUSTERS; LUMINOSITY FUNCTION; SPIRAL GALAXIES; ADVANCED CAMERA; MILKY-WAY; SYSTEMS; FIELD; M31; IDENTIFICATION AB Hubble Space Telescope Advanced Camera for Surveys (ACS) images are used to identify and study star cluster candidates in the nearby spiral galaxy M101. About 3000 round, slightly resolved cluster candidates are identified in 10 ACS pointings covering an area of 106 arcmin(2). The cluster candidates' color and size distributions are consistent with those of star clusters in other nearby spirals. The majority of the M101 candidates are blue and more likely to be associated with the galaxy's spiral arms, implying that they are young. The galaxy-luminosity-normalized number of young massive clusters in M101 is similar to that found in other spirals, as is the cluster density at a fiducial absolute magnitude. We confirm a previous finding that M101 has a large number of faint red star clusters: if these are old globular clusters, then this galaxy has a very large globular cluster population. More plausible is that the faint red clusters are reddened young clusters; their colors and luminosities are also consistent with this explanation. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Johns Hopkins Univ, Henry A Rowland Dept Phys & Astron, Baltimore, MD 21218 USA. NASA, Goddard Space Flight Ctr, Xray Astrophys Lab, Explorat Universe Div, Greenbelt, MD 20771 USA. RP Barmby, P (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM pbarmby@cfa.harvard.edu RI Barmby, Pauline/I-7194-2016 OI Barmby, Pauline/0000-0003-2767-0090 NR 36 TC 19 Z9 19 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 AUG PY 2006 VL 132 IS 2 BP 883 EP 890 DI 10.1086/505689 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 072WA UT WOS:000239702500036 ER PT J AU Maiorano, E Masetti, N Palazzi, E Savaglio, S Rol, E Vreeswijk, PM Pian, E Price, PA Peterson, BA Jelinek, M Amati, L Andersen, MI Castro-Tirado, AJ Ceron, JMC Postigo, AD Frontera, F Fruchter, AS Fynbo, JPU Gorosabel, J Henden, AA Hjorth, J Jensen, BL Klose, S Kouveliotou, C Masi, G Moller, P Nicastro, L Ofek, EO Pandey, SB Rhoads, J Tanvir, NR Wijers, RAMJ van den Heuvel, EPJ AF Maiorano, E. Masetti, N. Palazzi, E. Savaglio, S. Rol, E. Vreeswijk, P. M. Pian, E. Price, P. A. Peterson, B. A. Jelinek, M. Amati, L. Andersen, M. I. Castro-Tirado, A. J. Cern, J. M. Castro de Ugarte Postigo, A. Frontera, F. Fruchter, A. S. Fynbo, J. P. U. Gorosabel, J. Henden, A. A. Hjorth, J. Jensen, B. L. Klose, S. Kouveliotou, C. Masi, G. Moller, P. Nicastro, L. Ofek, E. O. Pandey, S. B. Rhoads, J. Tanvir, N. R. Wijers, R. A. M. J. van den Heuvel, E. P. J. TI Physics of the GRB 030328 afterglow and its environment SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE gamma rays : bursts; radiation mechanisms : non-thermal; line : identification; cosmology : observations ID GAMMA-RAY BURST; SOUTHERN SPECTROPHOTOMETRIC STANDARDS; 28 FEBRUARY 1997; LINEAR-POLARIZATION; OPTICAL AFTERGLOW; LIGHT CURVES; SUPERNOVA 2003DH; ERROR BOX; SPECTROSCOPY; EMISSION AB Aims. To investigate the physical nature of the afterglow emission. We report on the photometric, spectroscopic and polarimetric observations of the optical afterglow of Gamma-Ray Burst (GRB) 030328 detected by HETE-2. Methods. Photometric, spectroscopic and polarimetric monitoring of the optical afterglow. Results. Photometry, collected at 7 different telescopes, shows that a smoothly broken powerlaw decay, with indices alpha(1) = 0.76 +/- 0.03, alpha(2) = 1.50 +/- 0.07 and a break at t(b) = 0.48 +/- 0.03 days after the GRB, provides the best fit of the optical afterglow decline. This shape is interpreted as due to collimated emission, for which we determine a jet opening angle theta(jet) similar to 3 degrees.2. An achromatic bump starting around similar to 0.2 d after the GRB is possibly marginally detected in the optical light curves. Optical spectroscopy shows the presence of two rest-frame ultraviolet metal absorption systems at z = 1.5216 +/- 0.0006 and at z = 1.295 +/- 0.001, the former likely associated with the GRB host galaxy. Analysis of the absorption lines at z = 1.5216 suggests that the host of this GRB may be a Damped Lyman-alpha Absorber. The optical V-band afterglow appears polarized, with P = (2.4 +/- 0.6)% and theta = 170 degrees +/- 7 degrees, suggesting an asymmetric blastwave expansion. An X-ray-to-optical spectral flux distribution of the GRB 030328 afterglow was obtained at 0.78 days after the GRB and fitted using a broken powerlaw, with an optical spectral slope beta(opt) = 0.47 +/- 0.15, and an X-ray slope beta(X) = 1.0 +/- 0.2. Conclusions. The discussion of the results in the context of the "fireball model" shows that the preferred scenario for this afterglow is collimated structured jet with fixed opening angle in a homogeneous medium. C1 INAF, Ist Astrofis Spaziale & Fis Cosm Bologna, I-40129 Bologna, Italy. INAF, Osservatorio Astron Trieste, I-34131 Trieste, Italy. Univ Bologna, Dipartmento Astron, I-40126 Bologna, Italy. Johns Hopkins Univ, Baltimore, MD 21218 USA. Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England. European So Observ, Santiago 19, Chile. Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. Australian Natl Univ, Res Sch Astron & Astrophys, Weston, ACT 2611, Australia. CSIC, Inst Astrofis Andalucia, E-18080 Granada, Spain. Inst Astrophys, D-14482 Potsdam, Germany. Univ Copenhagen, Dark Cosmol Ctr, Niels Bohr Inst, DK-2100 Copenhagen O, Denmark. Univ Ferrara, Dipartimento Fis, I-44100 Ferrara, Italy. Space Telescope Sci Inst, Baltimore, MD 21218 USA. Univ Space Res Assoc, US Naval Observ, Flagstaff, AZ 86002 USA. Thuringer Landessternwarte Tautenburg, D-07778 Tautenburg, Germany. NASA, MSFC, Huntsville, AL 35812 USA. Univ Roma Tor Vergata, Dipartimento Fis, I-00133 Rome, Italy. European So Observ, D-85748 Garching, Germany. Tel Aviv Univ, Sch Phys & Astron, IL-69978 Tel Aviv, Israel. Tel Aviv Univ, Wise Observ, IL-69978 Tel Aviv, Israel. ARIES Observ, Naini Tal 263129, Uttaranchal, India. Univ Hertfordshire, Dept Phys Sci, Hatfield AL10 9AB, Herts, England. Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1098 SJ Amsterdam, Netherlands. RP Maiorano, E (reprint author), INAF, Ist Astrofis Spaziale & Fis Cosm Bologna, Via Gobetti 101, I-40129 Bologna, Italy. EM maiorano@iasfbo.inaf.it RI Fynbo, Johan/L-8496-2014; Nicastro, Luciano/F-5866-2015; Palazzi, Eliana/N-4746-2015; Amati, Lorenzo/N-5586-2015; Jelinek, Martin/E-5290-2016; Hjorth, Jens/M-5787-2014; Jensen, Brian Lindgren/E-1275-2015 OI Wijers, Ralph/0000-0002-3101-1808; Palazzi, Eliana/0000-0002-8691-7666; Savaglio, Sandra/0000-0003-2354-3238; de Ugarte Postigo, Antonio/0000-0001-7717-5085; Masetti, Nicola/0000-0001-9487-7740; Pian, Elena/0000-0001-8646-4858; Fynbo, Johan/0000-0002-8149-8298; Nicastro, Luciano/0000-0001-8534-6788; Amati, Lorenzo/0000-0001-5355-7388; Jelinek, Martin/0000-0003-3922-7416; Castro-Tirado, A. J./0000-0003-2999-3563; Hjorth, Jens/0000-0002-4571-2306; Jensen, Brian Lindgren/0000-0002-0906-9771 NR 79 TC 12 Z9 12 U1 1 U2 2 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD AUG PY 2006 VL 455 IS 2 BP 423 EP U13 DI 10.1051/0004-6361:20054728 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 070XM UT WOS:000239560000009 ER PT J AU Vanzella, E Cristiani, S Dickinson, M Kuntschner, H Nonino, M Rettura, A Rosati, P Vernet, J Cesarsky, C Ferguson, HC Fosbury, RAE Giavalisco, M Grazian, A Haase, J Moustakas, LA Popesso, P Renzini, A Stern, D AF Vanzella, E. Cristiani, S. Dickinson, M. Kuntschner, H. Nonino, M. Rettura, A. Rosati, P. Vernet, J. Cesarsky, C. Ferguson, H. C. Fosbury, R. A. E. Giavalisco, M. Grazian, A. Haase, J. Moustakas, L. A. Popesso, P. Renzini, A. Stern, D. CA GOODS Team TI The great observatories origins deep survey - VLT/FORS2 spectroscopy in the GOODS-South Field: Part II SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE cosmology : observations; cosmology : large scale structure of Universe; Galaxy : general ID TULLY-FISHER RELATION; GALAXIES; REDSHIFT; CONSTRAINTS; EVOLUTION; SPECTRA AB Aims. We present the second campaign of the ESO/GOODS program of spectroscopy of faint galaxies in the GOODS-South field. Methods. Objects were selected as candidates for VLT/FORS2 observations primarily based on the expectation that the detection and measurement of their spectral features would benefit from the high throughput and spectral resolution of FORS2. The reliability of the redshift estimates is assessed using the redshift-magnitude and color-redshift diagrams and comparing the results with public data. Results. 807 spectra of 652 individual targets have been obtained in service mode with the FORS2 spectrograph at the ESO/VLT, providing 501 redshift determinations. The typical redshift uncertainty is estimated to be sigma(z) similar or equal to 0.001. Galaxies have been selected adopting three different color criteria and using the photometric redshifts. The resulting redshift distribution typically spans two redshift domains: from z = 0.5 to 2 and z = 3.5 to 6.2. In particular, 94 B-435-, V-606-, i(775)- "dropout" Lyman break galaxies have been observed, yielding redshifts for 65 objects in the interval 3.4 < z < 6.2. Three sources have been serendipitously discovered in the redshift interval 4.8 < z < 5.5. Together with the previous release, 930 sources have now been observed and 724 redshift determinations have been carried out. The reduced spectra and the derived redshifts are released to the community through the ESO web page http://www.eso.org/science/goods/. Large scale structures are clearly detected at z similar or equal to 0.666, 0.734, 1.096, 1.221, 1.300, and 1.614. A sample of 34 sources with tilted [OII] 3727 emission has been identified, 32 of them in the redshift range 0.9 < z < 1.5. C1 Osserv Astron Trieste, INAF, I-40131 Trieste, Italy. Natl Opt Astron Observ, Tucson, AZ 85726 USA. ECF, ST, D-85748 Garching, Germany. Space Telescope Sci Inst, Baltimore, MD 21218 USA. European So Observ, D-85748 Garching, Germany. Univ Paris 11, F-91405 Orsay, France. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. Astron Observ Padova, INAF, I-35122 Padua, Italy. Osserv Astron Roma, INAF, I-00040 Rome, Italy. RP Vanzella, E (reprint author), Osserv Astron Trieste, INAF, Via GB Tiepolo 11, I-40131 Trieste, Italy. EM vanzella@oats.inaf.it OI Fosbury, Robert/0000-0001-9975-8003; Nonino, Mario/0000-0001-6342-9662; Cristiani, Stefano/0000-0002-2115-5234; Kuntschner, Harald/0000-0002-2768-1198; Vernet, Joel/0000-0002-8639-8560; Vanzella, Eros/0000-0002-5057-135X; Moustakas, Leonidas/0000-0003-3030-2360 NR 30 TC 170 Z9 170 U1 0 U2 4 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 AUG PY 2006 VL 454 IS 2 BP 423 EP 435 DI 10.1051/0004-6361:20054796 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 063FW UT WOS:000239004300032 ER PT J AU La Parola, V Mangano, V Fox, D Zhang, B Krimm, HA Cusumano, G Mineo, T Burrows, DN Barthelmy, S Campana, S Capalbi, M Chincarini, G Gehrels, N Giommi, P Marshall, FE Meszaros, P Moretti, A O'Brien, PT Palmer, DM Perri, M Romano, P Tagliaferri, G AF La Parola, V. Mangano, V. Fox, D. Zhang, B. Krimm, H. A. Cusumano, G. Mineo, T. Burrows, D. N. Barthelmy, S. Campana, S. Capalbi, M. Chincarini, G. Gehrels, N. Giommi, P. Marshall, F. E. Meszaros, P. Moretti, A. O'Brien, P. T. Palmer, D. M. Perri, M. Romano, P. Tagliaferri, G. TI GRB 051210: Swift detection of a short gamma ray burst SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE gamma rays : bursts; X-rays : bursts ID AFTERGLOWS; TELESCOPE; FLARES; GRB-050709; MISSION; GALAXY AB Aims. The short/hard GRB 051210 was detected and located by the Swift-BAT instrument and rapidly pointed towards by the narrow field instruments. The XRT was able to observe a bright, rapidly fading X-ray emission. We present the analysis of the prompt and afterglow emission of this event. Methods. The BAT spectrum is a power-law with photon index 1.0 +/- 0.3. The X-ray light curve decays with slope -2.58 +/- 0.11 and shows a small flare in the early phases. The spectrum can be described with a power law with photon index 1.54 +/- 0.16 and absorption (7.5(-3.2)(+4.3)) x 10(20) cm(-2). Results. We find that the X-ray emission is consistent with the hypothesis that we are observing the curvature effect of a GRB that occurred in a low density medium, with no detectable afterglow attributable to an external shock. We estimate the density of the circumburst medium to be lower than 3 x 10(-3) cm(-3). We also discuss different hypothesis on the possible origin of the flare. C1 INAF, Palermo, Italy. Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. Univ Nevada, Dept Phys, Las Vegas, NV 89154 USA. NASA Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Univ Space Res Assoc, Columbia, MD 21044 USA. INAF, Osserv Astron Brera, I-23807 Merate, Italy. ASI Sci Data Ctr, I-00044 Frascati, Italy. Univ Milan, Dipartimento Fis, I-20126 Milan, Italy. Penn State Univ, Dept Phys, University Pk, PA 16802 USA. Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England. Los Alamos Natl Lab, Los Alamos, NM 87545 USA. RP La Parola, V (reprint author), INAF, Palermo, Italy. EM laparola@ifc.inaf.it RI Barthelmy, Scott/D-2943-2012; Gehrels, Neil/D-2971-2012; OI Mineo, Teresa/0000-0002-4931-8445; giommi, paolo/0000-0002-2265-5003; Cusumano, Giancarlo/0000-0002-8151-1990; moretti, alberto/0000-0002-9770-0315; Perri, Matteo/0000-0003-3613-4409; La Parola, Valentina/0000-0002-8087-6488; Tagliaferri, Gianpiero/0000-0003-0121-0723 NR 55 TC 30 Z9 30 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 AUG PY 2006 VL 454 IS 3 BP 753 EP 757 DI 10.1051/0004-6361:20065083 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 064WQ UT WOS:000239121200012 ER PT J AU Markowitz, A Reeves, JN Braito, V AF Markowitz, A. Reeves, J. N. Braito, V. TI FeK emission and absorption in the XMM-epic spectrum of the Seyfert galaxy IC 4329a SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : active; galaxies : individual (IC 4329a); galaxies : Seyfert; X-rays : galaxies ID ACTIVE GALACTIC NUCLEI; RAY TIMING EXPLORER; IRON LINE-PROFILE; BLACK-HOLE MASS; ACCRETION DISK; BEPPOSAX OBSERVATION; NEWTON OBSERVATION; ALPHA PROFILE; REGION SIZES; COLD MATTER AB We present a detailed analysis of the XMM-Newton long-look of the Seyfert galaxy IC 4329a. The Fe K bandpass is dominated by two resolved peaks at 6.4 and 7.0 keV, consistent with neutral or near-neutral Fe K alpha and K beta emission. There is a prominent redward asymmetry in the 6.4 keV line, which could indicate emission from a Compton shoulder. Alternatively, models using dual relativistic disk lines are found to describe the emission profile well. A low-inclination, moderately relativistic dual disk-line model is possible if the contribution from narrow components, due to distant material, is small or absent. A high-inclination, moderately relativistic profile for each peak is possible if there are roughly equal contributions from both the broad and narrow components. Combining the XMM-Newton data with RXTE monitoring data, we explore the time-resolved spectral behavior on timescales from hours to 2 years. We find no strong evidence for variability of the Fe K line flux on any timescale, likely due to the minimal level of continuum variability. We detect, at high significance, a narrow absorption line at 7.68 keV. This feature is most likely due to Fe XXVI K alpha absorption blueshifted to similar to 0.1c relative to the systemic velocity, suggesting a high-velocity, highly ionized outflow component. As is often the case with similar outflows seen in high-luminosity quasars, the power associated with the outflow represents a substantial portion of the total energy budget of the AGN. The outflow could arise from a radiatively driven disk wind, or it may be in the form of a discrete, transient blob of ejected material. C1 NASA, Goddard Space Flight Ctr, Xray Astrophys Lab, Greenbelt, MD 20771 USA. Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. RP Markowitz, A (reprint author), NASA, Goddard Space Flight Ctr, Xray Astrophys Lab, Code 662, Greenbelt, MD 20771 USA. EM agm@milkyway.gsfc.nasa.gov; jnr@milkyway.gsfc.nasa.gov; vale@milkyway.gsfc.nasa.gov OI Braito, Valentina/0000-0002-2629-4989 NR 69 TC 59 Z9 59 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD AUG 1 PY 2006 VL 646 IS 2 BP 783 EP 800 DI 10.1086/505107 PN 1 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 072BK UT WOS:000239647400010 ER PT J AU Xu, CK Buat, V Iglesias-Paramo, J Takeuchi, TT Barlow, TA Bianchi, L Donas, J Forster, K Friedman, PG Heckman, TM Jelinsky, PN Lee, YW Madore, BF Malina, RF Martin, DC Milliard, B Morrissey, P Rich, RM Neff, SG Schiminovich, D Siegmund, OHW Small, T Szalay, AS Welsh, BY Wyder, TK Yi, S AF Xu, C. Kevin Buat, Veronique Iglesias-Paramo, Jorge Takeuchi, Tsutomu T. Barlow, Tom A. Bianchi, Luciana Donas, Jose Forster, Karl Friedman, Peter G. Heckman, Timothy M. Jelinsky, Patrick N. Lee, Young-Wook Madore, Barry F. Malina, Roger F. Martin, D. Christopher Milliard, Bruno Morrissey, Patrick Rich, R. Michael Neff, Susan G. Schiminovich, David Siegmund, Oswald H. W. Small, Todd Szalay, Alex S. Welsh, Barry Y. Wyder, Ted K. Yi, Sukyoung TI Ultraviolet and far-infrared-selected star-forming galaxies at z=0: Differences and overlaps SO ASTROPHYSICAL JOURNAL LA English DT Article DE dust : extinction; galaxies : active; galaxies : luminosity function; galaxies : mass function; galaxies : starburst; infrared : galaxies; stars : formation; ultraviolet : galaxies ID LYMAN BREAK GALAXIES; LUMINOSITY FUNCTION; LOCAL UNIVERSE; STARBURST GALAXIES; NEARBY UNIVERSE; DUST EXTINCTION; FORMATION RATES; FORMATION HISTORY; ASTRONOMICAL DATA; REDSHIFT SURVEY AB We study two samples of local galaxies, one UV (GALEX) selected and the other FIR (IRAS) selected, to address the question of whether UV and FIR surveys see two sides ("bright'' and "dark'') of the star formation of the same population of galaxies or two different populations of star-forming galaxies. No significant difference between the L-tot (=L-60 + L-FUV) luminosity functions of the UV and FIR samples is found. In addition, after the correction for the "Malmquist bias'' (bias for flux-limited samples), the FIR-to-UV ratio versus L-tot relations of the two samples are consistent with each other. In the range of 9 less than or similar to log (L-tot/L-circle dot) less than or similar to 12, both can be approximated by a simple linear relation of log (L-60/L-FUV) = log (L-tot/L-circle dot) - 9.66. These are consistent with the hypothesis that the two samples represent the same population of star-forming galaxies, and their well-documented differences in L-tot and in FIR-to-UV ratio are due only to the selection effect. A comparison between the UV luminosity functions shows marginal evidence for a population of faint UV galaxies missing in the FIR-selected sample. The contribution from these "FIR-quiet'' galaxies to the overall UV population is insignificant, given that the K-band luminosity functions (i.e., the stellar mass functions) of the two samples do not show any significant difference. C1 CALTECH, Pasadena, CA 91125 USA. Astron Observ, Astrophys Lab, F-13012 Marseille, France. CSIC, Inst Astrofis Andalucia, E-18008 Granada, Spain. Tohoku Univ, Astron Inst, Aoba Ku, Sendai, Miyagi 9808578, Japan. Johns Hopkins Univ, Ctr Astrophys Sci, Baltimore, MD 21218 USA. Astrophys Lab, F-13376 Marseille 12, France. Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. Yonsei Univ, Ctr Space Astrophys, Seoul 120749, South Korea. Observ Carnegie Inst Washington, Pasadena, CA 91101 USA. CALTECH, NASA, IPAC Extragalact Database, Pasadena, CA 91125 USA. Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA. NASA, Goddard Space Flight Ctr, Astron & Solar Phys Lab, Greenbelt, MD 20771 USA. RP Xu, CK (reprint author), CALTECH, MS 405-47,1200 E Calif Blvd, Pasadena, CA 91125 USA. OI malina, roger/0000-0003-3399-3865; Iglesias-Paramo, Jorge/0000-0003-2726-6370 NR 46 TC 13 Z9 13 U1 0 U2 6 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD AUG 1 PY 2006 VL 646 IS 2 BP 834 EP 840 DI 10.1086/504974 PN 1 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 072BK UT WOS:000239647400013 ER PT J AU Roussel, H Helou, G Smith, JD Draine, BT Hollenbach, DJ Moustakas, J Spoon, HW Kennicutt, RC Rieke, GH Walter, F Armus, L Dale, DA Sheth, K Bendo, GJ Engelbracht, CW Gordon, KD Meyer, MJ Regan, MW Murphy, EJ AF Roussel, H. Helou, G. Smith, J. D. Draine, B. T. Hollenbach, D. J. Moustakas, J. Spoon, H. W. Kennicutt, R. C. Rieke, G. H. Walter, F. Armus, L. Dale, D. A. Sheth, K. Bendo, G. J. Engelbracht, C. W. Gordon, K. D. Meyer, M. J. Regan, M. W. Murphy, E. J. TI The opaque nascent starburst in NGC 1377: Spitzer SINGS observations SO ASTROPHYSICAL JOURNAL LA English DT Article DE dust, extinction; galaxies : evolution; galaxies : individual (NGC 1377); galaxies : ISM; galaxies : starburst; infrared : galaxies ID EFFECTIVE COLLISION STRENGTHS; INFRARED SPECTROGRAPH IRS; SYNCHROTRON-DEFICIENT GALAXIES; SPECTRAL ENERGY-DISTRIBUTIONS; STAR-FORMING GALAXIES; H II REGIONS; INTERSTELLAR DUST; SPACE-TELESCOPE; NEARBY GALAXIES; IRON PROJECT AB We analyze extensive data on NGC 1377 from the Spitzer Infrared Nearby Galaxies Survey (SINGS). Within the category of nascent starbursts that we previously selected as having infrared-to-radio continuum ratios in large excess of the average and containing hot dust, NGC 1377 has the largest infrared excess yet measured. Optical imaging reveals a morphological distortion suggestive of a recent accretion event. Infrared spectroscopy reveals a compact and opaque source dominated by a hot, self-absorbed continuum(tau similar to 20 in the 10 mu m silicate band). We provide physical evidence against nonstellar activity being the heating source. H II regions are detected through the single [Ne II] line, probing < 1% of the ionizing radiation. Not only is the optical depth in different gas and dust phases very high, but > 85% of ionizing photons are suppressed by dust. The only other detected emission features are molecular hydrogen lines, arguably excited mainly by shocks, besides photodissociation regions, and weak aromatic bands. The new observations support our interpretation in terms of an extremely young starburst (< 1 Myr). More generally, galaxies deficient in radio synchrotron emission are likely observed within a few Myr of the onset of a starburst and after a long quiescence, prior to the replenishment of the interstellar medium with cosmic rays. The similar infrared-radio properties of NGC 1377 and some infrared-luminous galaxies suggest that NGC 1377 constitutes an archetype that will be useful to better understand starburst evolution. Although rare locally because observed in a brief evolutionary stage, nascent starbursts may represent a nonnegligible fraction of merger-induced starbursts that dominate deep infrared counts. Since they differ dramatically from usual starburst templates, they have important consequences for the interpretation of deep surveys. C1 CALTECH, Pasadena, CA 91125 USA. Max Planck Inst Astron, D-69117 Heidelberg, Germany. Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. Princeton Univ, Princeton, NJ 08544 USA. NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. Cornell Univ, Ithaca, NY 14853 USA. Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. Univ Wyoming, Laramie, WY 82071 USA. Univ London Imperial Coll Sci Technol & Med, London SW7 2AZ, England. Space Telescope Sci Inst, Baltimore, MD 21218 USA. Yale Univ, New Haven, CT 06520 USA. RP Roussel, H (reprint author), CALTECH, Pasadena, CA 91125 USA. OI Draine, Bruce/0000-0002-0846-936X NR 86 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 EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD AUG 1 PY 2006 VL 646 IS 2 BP 841 EP 857 DI 10.1086/505038 PN 1 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 072BK UT WOS:000239647400014 ER PT J AU Teegarden, BJ Watanabe, K AF Teegarden, B. J. Watanabe, K. TI A comprehensive search for gamma-ray lines in the first year of data from the INTEGRAL spectrometer SO ASTROPHYSICAL JOURNAL LA English DT Article DE gamma rays : observations ID POSITRON-ANNIHILATION RADIATION; GALACTIC-CENTER REGION; SOLAR-FLARES; EMISSION; SPI; AL-26; NUCLEOSYNTHESIS; SUPERNOVAE; DISCOVERY; SN-1987A AB We have carried out an extensive search for gamma-ray lines in the first year of public data from the spectrometer (SPI) on the INTEGRAL mission. INTEGRAL has spent a large fraction of its observing time in the Galactic plane with particular concentration in the Galactic center (GC) region (similar to 3 Ms in the first year). Hence the most sensitive search regions are in the Galactic plane and center. The phase space of the search spans the energy range 20-8000 keV and line widths from 0 to 1000 keV (FWHM). It includes both diffuse and pointlike emission. We have searched for variable emission on timescales down to similar to 1000 s. Diffuse emission has been searched for on a range of different spatial scales from similar to 20 degrees (the approximate field of view of the spectrometer) up to the entire Galactic plane. Our search procedures were verified by the recovery of the known gamma-ray lines at 511 and 1809 keV at the appropriate intensities and significances. We find no evidence for any previously unknown gamma-ray lines. The upper limits range from a few x 10(-5) to a few x 10(-2) cm(-2) s(-1) depending on line width, energy, and exposure; regions of strong instrumental background lines were excluded from the search. Comparison is made between our results and various prior predictions of astrophysical lines. C1 NASA, Goddard Space Flight Ctr, Explorat Universe Div, Greenbelt, MD 20771 USA. Univ Maryland, College Pk, MD 20742 USA. RP Teegarden, BJ (reprint author), NASA, Goddard Space Flight Ctr, Explorat Universe Div, Greenbelt, MD 20771 USA. NR 78 TC 21 Z9 21 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 AUG 1 PY 2006 VL 646 IS 2 BP 965 EP 981 DI 10.1086/504967 PN 1 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 072BK UT WOS:000239647400024 ER PT J AU Bryden, G Beichman, CA Rieke, GH Stansberry, JA Stapelfeldt, KR AF Bryden, G. Beichman, C. A. Rieke, G. H. Stansberry, J. A. Stapelfeldt, K. R. TI Spitzer MIPS limits on asteroidal dust in the pulsar planetary system PSR B1257+12 SO ASTROPHYSICAL JOURNAL LA English DT Article DE circumstellar matter; infrared : stars; pulsars : individual ( PSR B1257+12) ID MULTIBAND IMAGING PHOTOMETER; MILLISECOND PULSARS; MAGNETOHYDRODYNAMIC MODEL; REDUCTION ALGORITHMS; CIRCUMSTELLAR DISKS; DEBRIS DISKS; PSR B1257+12; SEARCH; STARS; PROTOPLANETARY AB With the MIPS camera on Spitzer, we have searched for far-infrared emission from dust in the planetary system orbiting pulsar PSR B1257+12. With accuracies of 0.05 mJy at 24 mu m and 1.5 mJy at 70 mu m, photometric measurements find no evidence for emission at these wavelengths. These observations place new upper limits on the luminosity of dust with temperatures between 20 and 1000 K. They are particularly sensitive to dust temperatures of 100-200 K, for which they limit the dust luminosity to below 3 x 10(-5) of the pulsar's spin-down luminosity, 3 orders of magnitude better than previous limits. Despite these improved constraints on dust emission, an asteroid belt similar to the solar system's cannot be ruled out. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. CALTECH, Michelson Sci Ctr, Pasadena, CA 91125 USA. Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. RP Bryden, G (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. RI Stapelfeldt, Karl/D-2721-2012 NR 48 TC 23 Z9 23 U1 0 U2 3 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD AUG 1 PY 2006 VL 646 IS 2 BP 1038 EP 1042 DI 10.1086/504976 PN 1 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 072BK UT WOS:000239647400029 ER PT J AU Crepp, JR Ge, J Heuvel, ADV Miller, SP Kuchner, MJ AF Crepp, Justin R. Ge, Jian Heuvel, Andrew D. Vanden Miller, Shane P. Kuchner, Marc J. TI Laboratory testing of a Lyot coronagraph equipped with an eighth-order notch filter image mask SO ASTROPHYSICAL JOURNAL LA English DT Article DE circumstellar matter; planetary systems; techniques : high angular resolution ID ORDER ADAPTIVE OPTICS; PLANETS AB We have built a series of notch filter image masks that make the Lyot coronagraph less susceptible to low spatial frequency optical aberrations. In this paper we present experimental results of their performance in the lab using monochromatic light. Our tests show that these "eighth-order'' masks are resistant to tilt and focus alignment errors and can generate contrast levels of 2 x 10(-6) at 3 lambda/D and 6 x 10(-7) at 10 lambda/D without the use of corrective optics such as deformable mirrors. This work supports recent theoretical studies suggesting that eighth-order masks can provide the Terrestrial Planet Finder-Coronagraph with a large search area, high off-axis throughput, and a practical requisite pointing accuracy. C1 Univ Florida, Dept Astron, Gainesville, FL 32611 USA. NASA, Goddard Space Flight Ctr, Exoplanets & Stellar Astrophys Lab, Greenbelt, MD 20771 USA. RP Crepp, JR (reprint author), Univ Florida, Dept Astron, 211 Bryant Space Sci Ctr,POB 112055, Gainesville, FL 32611 USA. EM jcrepp@astro.ufl.edu; jge@astro.ufl.edu; avh@astro.ufl.edu; smiller@astro.ufl.edu; marc.kuchner@nasa.gov RI Kuchner, Marc/E-2288-2012 NR 18 TC 9 Z9 9 U1 0 U2 5 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 AUG 1 PY 2006 VL 646 IS 2 BP 1252 EP 1259 DI 10.1086/504977 PN 1 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 072BK UT WOS:000239647400048 ER PT J AU Fregeau, JM Larson, SL Miller, MC O'Shaughnessy, R Rasio, FA AF Fregeau, John M. Larson, Shane L. Miller, M. Coleman O'Shaughnessy, Richard Rasio, Frederic A. TI Observing IMBH-IMBH binary coalescences via gravitational radiation SO ASTROPHYSICAL JOURNAL LA English DT Article DE black hole physics; gravitational waves; stellar dynamics ID MASS BLACK-HOLES; YOUNG STAR-CLUSTERS; SPACE-TELESCOPE EVIDENCE; RUNAWAY COLLISIONS; GLOBULAR-CLUSTERS; EVOLUTION; GALAXIES; M15; MERGERS; COUNTS AB Recent numerical simulations have suggested the possibility of forming double intermediate-mass black holes (IMBHs) via the collisional runaway scenario in young dense star clusters. The two IMBHs that formed would exchange into a common binary shortly after their birth and quickly inspiral and merge. Since space-borne gravitational wave (GW) observatories such as LISA will be able to see the late phases of their inspiral out to several gigaparsecs, and LIGO will be able to see the merger and ringdown out to similar distances, they represent potentially significant GW sources. In this Letter we estimate the rate at which LISA and LIGO will see their inspiral and merger in young star clusters, and we discuss the information that can be extracted from the observations. We find that LISA will likely see tens of IMBH-IMBH inspirals per year, while advanced LIGO could see similar to 10 merger and ringdown events per year, with both rates strongly dependent on the distribution of cluster masses and densities. C1 Northwestern Univ, Dept Phys & Astron, Evanston, IL 60208 USA. Penn State Univ, Ctr Gravitat Wave Phys, University Pk, PA 16802 USA. Univ Maryland, Dept Astron, College Pk, MD 20742 USA. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Fregeau, JM (reprint author), Northwestern Univ, Dept Phys & Astron, Evanston, IL 60208 USA. EM fregeau@alum.mit.edu; shane@gravity.psu.edu; miller@astro.umd.edu; oshaughn@northwestern.edu; rasio@northwestern.edu RI Larson, Shane/E-8576-2010; OI O'Shaughnessy, Richard/0000-0001-5832-8517 NR 35 TC 59 Z9 59 U1 0 U2 3 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD AUG 1 PY 2006 VL 646 IS 2 BP L135 EP L138 DI 10.1086/507106 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 072BL UT WOS:000239647500012 ER PT J AU Giannakis, O Harlaftis, ET Niarchos, PG Kitsionas, S Barwig, H Still, M Rutten, RGM AF Giannakis, O. Harlaftis, E. T. Niarchos, P. G. Kitsionas, S. Barwig, H. Still, M. Rutten, R. G. M. TI Mapping of the disc structure of the neutron star X-ray binary X1822-371 SO ASTROPHYSICS AND SPACE SCIENCE LA English DT Article; Proceedings Paper CT Conference on Close Binary Stars in the 21st Century - New Opportunities and Challenges CY JUN 27, 2005-JUN 30, 2006 CL Syros, GREECE DE low-mass X-ray binaries; X1822-371 AB We report the results of simultaneous optical/ X-ray observations of X1822-371 at 0.1 second time resolution. The preliminary analysis finds no correlation between the optical/X-ray light curves. We aim to constrain the vertical structure and radius of the accretion disc. C1 Natl Observ Athens, GR-11810 Athens, Greece. Univ Athens, Dept Astrophys Astron & Mech, GR-15784 Athens, Greece. Astrophys Inst Postdam, D-14482 Potsdam, Germany. Univ Sternwarte Munchen, D-81679 Munich, Germany. NASA, Goddard Space Flight Ctr, Univ Space Res Assoc, Greenbelt, MD 20771 USA. Isaac Newton Grp Telescopes, E-38700 Santa Cruz de La Palma, Spain. RP Giannakis, O (reprint author), Natl Observ Athens, POB 20048, GR-11810 Athens, Greece. RI Giannakis, Omiros/K-4420-2013 OI Giannakis, Omiros/0000-0002-2470-1042 NR 7 TC 0 Z9 0 U1 1 U2 2 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0004-640X J9 ASTROPHYS SPACE SCI JI Astrophys. Space Sci. PD AUG PY 2006 VL 304 IS 1-4 BP 321 EP 322 DI 10.1007/s10509-006-9142-8 PG 2 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 109BX UT WOS:000242284000081 ER PT J AU Koch, D Borucki, W Basri, G Brown, T Caldwell, D Christensen-Dalsgaard, J Cochran, W Dunham, E Gautier, TN Geary, J Gilliland, R Jenkins, J Kondo, Y Latham, D Lissauer, J Monet, D AF Koch, D. Borucki, W. Basri, G. Brown, T. Caldwell, D. Christensen-Dalsgaard, J. Cochran, W. Dunham, E. Gautier, T. N. Geary, J. Gilliland, R. Jenkins, J. Kondo, Y. Latham, D. Lissauer, J. Monet, D. TI The Kepler mission: Astrophysics and eclipsing binaries SO ASTROPHYSICS AND SPACE SCIENCE LA English DT Article; Proceedings Paper CT Conference on Close Binary Stars in the 21st Century - New Opportunities and Challenges CY JUN 27, 2005-JUN 30, 2006 CL Syros, GREECE DE extra-solar planets; planet detection; eclipsing binaries; precision photometry AB The Kepler Mission is a photometric space mission that will continuously observe a single 100 square degree field of view (FOV) of the sky of more than 100,000 stars in the Cygnus-Lyra region for four or more years with a precision of 14 parts per million (ppm) for a 6.5 hour integration including shot noise for a twelfth magnitude star. The primary goal of the mission is to detect Earth-size planets in the habitable zone of solar-like stars. In the process, many eclipsing binaries (EB) will also be detected. Prior to launch, the stellar characteristics will have been determined for all the stars in the FOV with K < 14.5. As part of the verification process, stars with transits (about 5%) will need to have follow-up radial velocity observations performed to determine the component masses and thereby separate grazing eclipses caused by stellar companions from transits caused by planets. The result will be a rich database on EBs. The community will have access to the archive for uses such as for EB modeling of the high-precision light curves. A guest observer program is also planned for objects not already on the target list. C1 NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. Univ Calif Berkeley, Berkeley, CA 94720 USA. High Altitude Observ, Boulder, CO 80307 USA. SETI Inst, Mountain View, CA 94043 USA. Univ Aarhus, DK-8000 Aarhus C, Denmark. Univ Texas, Austin, TX 78712 USA. Lowell Observ, Flagstaff, AZ 86001 USA. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. Space Telescope Sci Inst, Baltimore, MD 21218 USA. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. USN Observ, Flagstaff, AZ 86002 USA. RP Koch, D (reprint author), NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RI Caldwell, Douglas/L-7911-2014 OI Caldwell, Douglas/0000-0003-1963-9616 NR 8 TC 6 Z9 6 U1 0 U2 4 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0004-640X J9 ASTROPHYS SPACE SCI JI Astrophys. Space Sci. PD AUG PY 2006 VL 304 IS 1-4 BP 391 EP 395 DI 10.1007/s10509-006-9149-1 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 109BX UT WOS:000242284000098 ER PT J AU Conkin, J Sung, HG Feiveson, AH AF Conkin, Johnny Sung, Hsi-Guang Feiveson, Alan H. TI A latent class model to assess error rates in diagnosis of altitude decompression sickness SO AVIATION SPACE AND ENVIRONMENTAL MEDICINE LA English DT Article DE aviator decompression sickness; false-positive rate; false-negative rate; inter-rater agreement; positive predictive value; negative predictive value; gold standard ID INTRAVASCULAR BUBBLE SIGNALS; AGREEMENT; ILLNESS AB Background: Prospective testing of denitrogenation protocols to reduce the risk of decompression sickness (DCS) in astronauts requires pre-defined accept and reject criteria. We assume that the end-point of a test, the presence or absence of signs and symptoms attributable to DCS, is unequivocal. However, diagnosis of DCS is not perfect, nor is there is a gold standard to assess diagnosis error rates. These error rates could cause consistent bias in the decision to accept or reject proposed protocols. We used a Latent Class Model (LCM) incorporating inter-rater agreement to estimate false-positive and negative rates of DCS diagnosis for each of six symptomatic (covariate) strata. Methods: Case descriptions from 135 reports collected since 1982 were available with 103 diagnosed as DCS (73.1%). There were 3 subsets of 45 descriptions that were randomly selected, information about the original diagnosis omitted, and were sent to 15 physicians (raters), all experts in altitude DCS. Subsets were diagnosed for DCS by either four, five, or six raters. We then used a LCM to estimate false-positive and false-negative error rates for the original NASA test diagnosis, even though a gold standard was not available. Results: Estimates of false-positive rates in the NASA diagnoses ranged from 13% to 83% and from 1% to 32% for false-negative rates over the six strata of symptomatic response variables. Conclusions: Our findings suggest that use of current DCS diagnostic outcomes as if they were error free would likely produce an inflated rejection rate of acceptable protocols in future testing if adjustments are not made. C1 NASA, Lyndon B Johnson Space Ctr, Human Adaptat & Countermeasures Off, Environm Physiol Lab, Houston, TX 77058 USA. Baylor Coll Med, Natl Space Biomed Res Inst, Houston, TX 77030 USA. RP Conkin, J (reprint author), NASA, Lyndon B Johnson Space Ctr, Human Adaptat & Countermeasures Off, Environm Physiol Lab, SK2,2101 NASA Rd 1, Houston, TX 77058 USA. EM jconkin@ems.jsc.nasa.gov NR 12 TC 4 Z9 4 U1 0 U2 0 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 AUG PY 2006 VL 77 IS 8 BP 816 EP 824 PG 9 WC Public, Environmental & Occupational Health; Medicine, General & Internal; Sport Sciences SC Public, Environmental & Occupational Health; General & Internal Medicine; Sport Sciences GA 070GC UT WOS:000239507300005 PM 16909875 ER PT J AU Rafiq, A Hummel, R Lavrentyev, V Derry, W Williams, D Merrell, RC AF Rafiq, Azhar Hummel, Russ Lavrentyev, Vladimir Derry, William Williams, David Merrell, Ronald C. TI Microgravity effects on fine motor skills: Tying surgical knots during parabolic flight SO AVIATION SPACE AND ENVIRONMENTAL MEDICINE LA English DT Article DE laparoscopic surgical simulation; medical care; training; surgery in space; laparoscopic surgery ID SPACEFLIGHT; SURGERY AB Introduction: The health provider on a space exploration mission cannot evacuate a patient to Earth. Contingency plans for medical intervention must be designed for autonomy. This study measured the effect of microgravity on performance of fine motor skills such as basic surgical tasks. Methods: Eight subjects, six with medical and two with non-medical backgrounds, were evaluated during parabolic microgravity flights aboard NASA's KC-135. We evaluated their skill in tying surgical knots on simulated skin made of silicone using standard techniques for minimally invasive surgery. LabView (R) software was developed to archive forces applied to the laparoscopic tool handles during knot-tying. Studies were controlled for medication (ScopeDex) and the aircraft environment. Results: Ail participants completed the tests successfully. The data indicated that increased force was applied to the instruments and knot quality decreased during flight compared with ground control sessions. Conclusion: Specific metrics of surgical task performance are essential in developing education modules for providers of medical care during exploration-class missions. C1 Virginia Commonwealth Univ, Dept Surg, Med Informat & Technol Applicat Consortium, Richmond, VA 23298 USA. NASA, Lyndon B Johnson Space Ctr, Astronaut Off, Houston, TX 77058 USA. Yale Univ, New Haven, CT USA. RP Rafiq, A (reprint author), Virginia Commonwealth Univ, Dept Surg, Med Informat & Technol Applicat Consortium, 1101 E Marshall St,POB 980480, Richmond, VA 23298 USA. EM arafiq@vcu.edu NR 12 TC 8 Z9 8 U1 1 U2 4 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 AUG PY 2006 VL 77 IS 8 BP 852 EP 856 PG 5 WC Public, Environmental & Occupational Health; Medicine, General & Internal; Sport Sciences SC Public, Environmental & Occupational Health; General & Internal Medicine; Sport Sciences GA 070GC UT WOS:000239507300011 PM 16909881 ER PT J AU Biennier, L Benidar, A Salama, F AF Biennier, Ludovic Benidar, Abdessamad Salama, Farid TI Flow dynamics of a pulsed planar expansion SO CHEMICAL PHYSICS LA English DT Article DE computational flow dynamics; pulsed planar expansions; pulsed discharge nozzles; astrochemistry; molecular spectroscopy; polycyclic aromatic hydrocarbons ID POLYCYCLIC AROMATIC-HYDROCARBONS; RING-DOWN SPECTROSCOPY; CAVITY RING; INFRARED-SPECTROSCOPY; DISCHARGE NOZZLE; MOLECULES; IONIZATION; RADICALS; BANDS; C-70 AB Plasma expansion sources are popular in molecular spectroscopy and in astrochemistry because they generate cold radicals and ions in detectable amounts. The dynamics of a planar flow generated by a pulsed discharge slit nozzle (PDN) have been numerically investigated for a variety of carrier gases seeded with various molecular species. The determination of the bulk flow characteristics is key to a comprehensive modeling of the plasma that is produced in PDN sources. It is found that the flow is established and stabilized within 75 and 25 mu s when Ar and He are used as carrier gases, respectively. The residence time in the inter-electrode active region is found to be considerably shorter with He than with Ar gas carrier. The detection signal observed upon injection of astrochemical species such as polycylic aromatic hydrocarbons (PAHs) in moderate amounts in the carrier gas exhibits a non linear relation with the initial PAH concentration in the reservoir which is governed by the temperature. The local temperature along the flow axis can be predicted from the initial conditions using the isentropic equation. However, the local pressure and density behavior diverge significantly from an isentropic flow. Finally, implications for the characteristics of the plasma expansion are discussed to help design future laboratory simulations. (c) 2006 Elsevier B.V. All rights reserved. C1 Univ Rennes 1, Lab Phys Atom Lasers Mol & Surface, Rennes, France. NASA, Ames Res Ctr, Div Space Sci, Moffett Field, CA 94035 USA. RP Biennier, L (reprint author), Univ Rennes 1, Lab Phys Atom Lasers Mol & Surface, Rennes, France. EM ludovic.biennier@univ-rennes1.fr RI Salama, Farid/A-8787-2009; Biennier, Ludovic/O-1618-2014; benidar, abdessamad/O-1624-2014 OI Salama, Farid/0000-0002-6064-4401; NR 31 TC 12 Z9 12 U1 1 U2 11 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0301-0104 J9 CHEM PHYS JI Chem. Phys. PD AUG 1 PY 2006 VL 326 IS 2-3 BP 445 EP 457 DI 10.1016/j.chemphys.2006.03.016 PG 13 WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical SC Chemistry; Physics GA 068NH UT WOS:000239380700023 ER PT J AU Neudeck, PG Trunek, AJ Spry, DJ Powell, JA Du, H Skowronski, M Huang, XR Dudley, M AF Neudeck, Philip G. Trunek, Andrew J. Spry, David J. Powell, J. Anthony Du, Hui Skowronski, Marek Huang, Xian Rong Dudley, Michael TI CVD growth of 3C-SiC on 4H/6H mesas SO CHEMICAL VAPOR DEPOSITION LA English DT Article DE 3C-SiC; dislocations; heteroepitaxy; mesas; surface steps ID FREE-SURFACE HETEROEPITAXY; SILICON-CARBIDE; EPITAXIAL-GROWTH; POWER DEVICES; 4H-SIC MESAS; FILMS; DEFECTS; LAYERS; 6H-SIC(0001); CANTILEVERS AB This article describes growth and characterization of the highest quality reproducible 3C-SiC heteroepitaxial films ever reported. By properly nucleating 3C-SiC growth on top of perfectly on-axis (0001) 4H-SiC mesa surfaces completely free of atomic scale steps and extended defects, growth of 3C-SiC mesa heterofilms completely free of extended crystal defects can be achieved. In contrast, nucleation and growth of 3C-SiC mesa heterofilms on top of 4H-SiC mesas with atomic-scale steps always results in numerous observable dislocations threading through the 3C-SiC epilayer. High-resolution X-ray diffraction (HRXRD) and high resolution cross-sectional transmission electron microscopy (HRXTEM) measurements indicate non-trivial, in-plane, lattice mismatch between the 3C and 4H layers. This mismatch is somewhat relieved in the step-free mesa case via misfit dislocations confined to the 3C/4H interfacial region without dislocations threading into the overlying 3C-SiC layer. These results indicate that the presence or absence of steps at the 3C/4H heteroepitaxial interface critically impacts the quality, defect structure, and relaxation mechanisms of single-crystal heteroepitaxial 3C-SiC films. C1 NASA, Glenn Res Ctr Lewis Field, Cleveland, OH 44135 USA. NASA, Glenn Res Ctr, OAI, Cleveland, OH 44135 USA. Sets Inc, NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. Carnegie Mellon Univ, Dept Mat Sci & Engn, Pittsburgh, PA 15213 USA. SUNY Stony Brook, Dept Mat Sci & Engn, Stony Brook, NY 11794 USA. RP Neudeck, PG (reprint author), NASA, Glenn Res Ctr Lewis Field, 21000 Brookpk Rd,MS 77-1, Cleveland, OH 44135 USA. EM Neudeck@nasa.qov RI Skowronski, Marek/A-8934-2011 OI Skowronski, Marek/0000-0002-2087-0068 NR 42 TC 43 Z9 43 U1 0 U2 17 PU WILEY-V C H VERLAG GMBH PI WEINHEIM PA PO BOX 10 11 61, D-69451 WEINHEIM, GERMANY SN 0948-1907 J9 CHEM VAPOR DEPOS JI Chem. Vapor Depos. PD AUG PY 2006 VL 12 IS 8-9 BP 531 EP 540 DI 10.1002/cvde.200506460 PG 10 WC Electrochemistry; Materials Science, Coatings & Films; Physics, Condensed Matter SC Electrochemistry; Materials Science; Physics GA 080XQ UT WOS:000240282200011 ER PT J AU Wyant, MC Bretherton, CS Bacmeister, JT Kiehl, JT Held, IM Zhao, M Klein, SA Soden, BJ AF Wyant, Matthew C. Bretherton, Christopher S. Bacmeister, Julio T. Kiehl, Jeffrey T. Held, Isaac M. Zhao, Ming Klein, Stephen A. Soden, Brian J. TI A comparison of low-latitude cloud properties and their response to climate change in three AGCMs sorted into regimes using mid-tropospheric vertical velocity SO CLIMATE DYNAMICS LA English DT Article ID GENERAL-CIRCULATION MODELS; LARGE-SCALE MODELS; COMMUNITY ATMOSPHERIC MODEL; RADIATION BUDGET EXPERIMENT; RELAXED ARAKAWA-SCHUBERT; SEA-SURFACE TEMPERATURE; STRATIFORM CLOUDS; MOIST CONVECTION; PART I; PARAMETERIZATION AB Low-latitude cloud distributions and cloud responses to climate perturbations are compared in near-current versions of three leading U.S. AGCMs, the NCAR CAM 3.0, the GFDL AM2.12b, and the NASA GMAO NSIPP-2 model. The analysis technique of Bony et al. (Clim Dyn 22:71-86, 2004) is used to sort cloud variables by dynamical regime using the monthly mean pressure velocity omega at 500 hPa from 30S to 30N. All models simulate the climatological monthly mean top-of-atmosphere longwave and shortwave cloud radiative forcing (CRF) adequately in all omega-regimes. However, they disagree with each other and with ISCCP satellite observations in regime-sorted cloud fraction, condensate amount, and cloud-top height. All models have too little cloud with tops in the middle troposphere and too much thin cirrus in ascent regimes. In subsidence regimes one model simulates cloud condensate to be too near the surface, while another generates condensate over an excessively deep layer of the lower troposphere. Standardized climate perturbation experiments of the three models are also compared, including uniform SST increase, patterned SST increase, and doubled CO2 over a mixed layer ocean. The regime-sorted cloud and CRF perturbations are very different between models, and show lesser, but still significant, differences between the same model simulating different types of imposed climate perturbation. There is a negative correlation across all general circulation models (GCMs) and climate perturbations between changes in tropical low cloud cover and changes in net CRF, suggesting a dominant role for boundary layer cloud in these changes. For some of the cases presented, upper-level clouds in deep convection regimes are also important, and changes in such regimes can either reinforce or partially cancel the net CRF response from the boundary layer cloud in subsidence regimes. This study highlights the continuing uncertainty in both low and high cloud feedbacks simulated by GCMs. C1 Univ Washington, Dept Atmospher Sci, Seattle, WA 98195 USA. NASA, Goddard Space Flight Ctr, Global Modeling & Assimilat Off, Greenbelt, MD 20771 USA. Natl Ctr Atmospher Res, Boulder, CO 80307 USA. NOAA, Geophys Fluid Dynam Lab, Princeton, NJ USA. Lawrence Livermore Natl Lab, Div Atmospher Sci, Livermore, CA USA. Univ Miami, Rosenstiel Sch Marine & Atmospher Sci, Div Meteorol & Phys Oceanog, Miami, FL 33149 USA. RP Wyant, MC (reprint author), Univ Washington, Dept Atmospher Sci, Box 351640, Seattle, WA 98195 USA. EM mwyant@atmos.washington.edu RI Zhao, Ming/C-6928-2014; Klein, Stephen/H-4337-2016 OI Klein, Stephen/0000-0002-5476-858X NR 44 TC 73 Z9 74 U1 0 U2 6 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0930-7575 EI 1432-0894 J9 CLIM DYNAM JI Clim. Dyn. PD AUG PY 2006 VL 27 IS 2-3 BP 261 EP 279 DI 10.1007/s00382-006-0138-4 PG 19 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 070CB UT WOS:000239496800009 ER PT J AU Salas, MD AF Salas, MD TI Some observations on grid convergence SO COMPUTERS & FLUIDS LA English DT Article AB It is claimed that current practices in grid convergence studies, particularly in the field of external aerodynamics, are flawed. The necessary conditions to properly establish grid convergence are presented. A theoretical model and a numerical example are used to demonstrate these ideas. It is shown that anomalously low or high observed convergence rates can be exhibited by otherwise well-behaved algorithms because of improper use of grid refinement ratios in different directions. (c) 2006 Elsevier Ltd. All rights reserved. C1 NASA, Langley Res Ctr, Hampton, VA 23681 USA. RP Salas, MD (reprint author), NASA, Langley Res Ctr, Mail Stop 499, Hampton, VA 23681 USA. EM m.d.salas@nasa.gov NR 12 TC 19 Z9 19 U1 0 U2 3 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0045-7930 J9 COMPUT FLUIDS JI Comput. Fluids PD AUG PY 2006 VL 35 IS 7 BP 688 EP 692 DI 10.1016/j.compfluid.2006.01.003 PG 5 WC Computer Science, Interdisciplinary Applications; Mechanics SC Computer Science; Mechanics GA 052PX UT WOS:000238246800005 ER PT J AU Reddy, DR Zaman, KBMQ AF Reddy, DR Zaman, KBMQ TI Computational study of effect of tabs on a jet in a cross flow SO COMPUTERS & FLUIDS LA English DT Article ID 3-DIMENSIONAL COMPRESSIBLE FLOW; AXISYMMETRICAL JET; VORTEX GENERATORS AB A three-dimensional viscous flow analysis is performed using a time-marching Reynolds-averaged Navier-Stokes code for the case of a jet in a cross flow with a delta tab placed on the windward side of the jet to inhibit mixing for film cooling applications. The flow configuration which was previously studied experimentally, involved a jet discharging normally from the floor of the wind tunnel test section into the cross flow with a momentum ratio (jet/cross-flow) of 36. The computed results are compared with the experimental data which include streamwise velocity and vorticity distributions at various axial locations downstream of the jet. The computational results show reasonably good agreement with the experimental data. (c) 2006 Elsevier Ltd. All rights reserved. C1 NASA, John H Glenn Res Ctr, Cleveland, OH 44135 USA. RP Reddy, DR (reprint author), NASA, John H Glenn Res Ctr, Cleveland, OH 44135 USA. NR 28 TC 4 Z9 4 U1 1 U2 9 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0045-7930 J9 COMPUT FLUIDS JI Comput. Fluids PD AUG PY 2006 VL 35 IS 7 BP 712 EP 723 DI 10.1016/j.compfluid.2006.01.011 PG 12 WC Computer Science, Interdisciplinary Applications; Mechanics SC Computer Science; Mechanics GA 052PX UT WOS:000238246800008 ER PT J AU Reddy, DR Sree, D AF Reddy, DR Sree, D TI Computational study of flow in a rocket-based combined cycle (RBCC) engine inlet SO COMPUTERS & FLUIDS LA English DT Article AB A two-dimensional axisymmetric viscous flow analysis of a rocket-based combined cycle (RBCC) engine inlet is performed using a time-marching numerical scheme to solve the Reynolds-averaged Navier-Stokes equations. The flow configuration is a subscale model of the engine inlet which was previously tested in the 1X1 supersonic wind tunnel at NASA Glenn Research Center. The computed results are compared with the experimental data which include static pressure profiles along the centerbody and the cowl surface of the inlet. The computational results show a reasonably good agreement with the experimental data. (c) 2006 Elsevier Ltd. All rights reserved. C1 NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. Tuskegee Univ, Tuskegee, AL 36088 USA. RP Reddy, DR (reprint author), NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. NR 23 TC 1 Z9 1 U1 4 U2 18 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0045-7930 J9 COMPUT FLUIDS JI Comput. Fluids PD AUG PY 2006 VL 35 IS 7 BP 724 EP 732 DI 10.1016/j.compfluid.2006.01.010 PG 9 WC Computer Science, Interdisciplinary Applications; Mechanics SC Computer Science; Mechanics GA 052PX UT WOS:000238246800009 ER PT J AU Conway, G AF Conway, Greg TI STAT3-dependent pathfinding and control of axonal branching and target selection SO DEVELOPMENTAL BIOLOGY LA English DT Article DE STAT3; transcription factor; pathfinding; motoneuron; zebrafish ID CILIARY NEUROTROPHIC FACTOR; STAT3 SIGNALING PATHWAY; BORDER CELL-MIGRATION; RECEPTOR-ALPHA-COMPONENT; MESSENGER-RNA EXPRESSION; EMBRYONIC ZEBRAFISH; NEURITE OUTGROWTH; JAK/STAT PATHWAY; C-JUN; GENE-EXPRESSION AB Signal transducers and transcription factors are used in common for developmental cell migration, vasculogenesis, branching morphogenesis, as well as neuronal pathfinding. STAT3, a transcription factor, has been shown to function in all of these processes except neuronal pathfinding. Here, it is shown that STAT3 also facilitates this process. Elimination of STAT3 signaling results in half of zebrafish Cap motoneurons stalling along their ventral pathfinding trajectory. Conversely, constitutive activation leads to precocious branching and redefines CaP axons as a responding population to dorsal guidance cues, resulting in bifurcated axons innervating normal ventral targets as well as additional dorsal muscle groups. These results are consistent with and highlight a fundamental role for STAT3 as a factor promoting cellular responses to guidance cues, not only in nonneural cells but also in pathfinding neurons. (c) 2006 Elsevier Inc. All rights reserved. C1 NASA, Ames Res Ctr, Div Life Sci, Moffett Field, CA 94035 USA. RP Conway, G (reprint author), NASA, Ames Res Ctr, Div Life Sci, MS239-11, Moffett Field, CA 94035 USA. EM gconway@mail.arc.nasa.gov NR 93 TC 15 Z9 15 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 0012-1606 J9 DEV BIOL JI Dev. Biol. PD AUG 1 PY 2006 VL 296 IS 1 BP 119 EP 136 DI 10.1016/j.ydbio.2006.04.444 PG 18 WC Developmental Biology SC Developmental Biology GA 068GD UT WOS:000239359800010 PM 16729994 ER PT J AU Seabloom, EW Williams, JW Slayback, D Stoms, DM Viers, JH Dobson, AP AF Seabloom, Eric W. Williams, John W. Slayback, Daniel Stoms, David M. Viers, Joshua H. Dobson, Andy P. TI Human impacts, plant invasion, and imperiled, plant species in California SO ECOLOGICAL APPLICATIONS LA English DT Article DE California, USA; dispersal; exotic plants; extinction; global biodiversity hotspot; habitat loss; invasive species; rare species; species richness; structural equation models ID UNITED-STATES; BIOLOGICAL INVASIONS; CLIMATE-CHANGE; DIVERSITY; PATTERNS; RICHNESS; BIODIVERSITY; COMPETITION; GRASSLAND; ECOSYSTEM AB Invasive species are one of the fastest growing conservation problems. These species homogenize the world's flora and fauna, threaten rare and endemic species, and impose large economic costs. Here, we examine the distribution of 834 of the more than 1000 exotic plant taxa that have become established in Califoriiia, USA. Total species richness increases with net primary productivity; however, the exotic flora is richest in low-lying coastal sites that harbor large numbers of imperiled species; while native diversity is highest in areas with high mean elevation. Weedy and invasive exotics are more tightly linked to the distribution of imperiled species than the overall pool of exotic species. Structural equation modeling suggests that while human activities, such as urbanization and agriculture, facilitate the initial invasion by exotic plants, exotics spread ahead of the front of human development into areas with high numbers of threatened native plants. The range sizes of exotic taxa are an order of magnitude smaller than for comparable native taxa. The current small range size of exotic species implies that California has a significant "invasion debt" that will be paid as exotic plants expand their range and spread throughout the state. C1 Oregon State Univ, Dept Zool, Corvallis, OR 97331 USA. Univ Wisconsin, Dept Geog, Madison, WI 53706 USA. NASA, Goddard Space Flight Ctr, Biospher Sci Branch, Sci Syst & Applicat Inc, Greenbelt, MD 20771 USA. Univ Calif Santa Barbara, Inst Computat Earth Syst Sci, Santa Barbara, CA 93106 USA. Univ Calif Davis, Dept Environm Sci & Policy, Davis, CA 95616 USA. Princeton Univ, Dept Ecol & Evolutionary Biol, Princeton, NJ 08544 USA. RP Seabloom, EW (reprint author), Oregon State Univ, Dept Zool, Corvallis, OR 97331 USA. EM seabloom@science.oregonstate.edu RI Slayback, Daniel/E-7465-2011; OI Seabloom, Eric/0000-0001-6780-9259 NR 63 TC 85 Z9 89 U1 6 U2 68 PU ECOLOGICAL SOC AMER PI WASHINGTON PA 1707 H ST NW, STE 400, WASHINGTON, DC 20006-3915 USA SN 1051-0761 J9 ECOL APPL JI Ecol. Appl. PD AUG PY 2006 VL 16 IS 4 BP 1338 EP 1350 DI 10.1890/1051-0761(2006)016[1338:HIPIAI]2.0.CO;2 PG 13 WC Ecology; Environmental Sciences SC Environmental Sciences & Ecology GA 073EV UT WOS:000239726700009 PM 16937802 ER PT J AU Zahnle, KJ AF Zahnle, Kevin J. TI Earth's earliest atmosphere SO ELEMENTS LA English DT Article DE Hadean Earth; Moon-forming impact; origin; evolution of the atmosphere; zircon ID EVOLUTION; OXYGEN; IMPACT; TEMPERATURES; MARS; GA AB The aftermath of the Moon-forming impact left Earth with a hot, CO2-rich steam atmosphere. Water oceans condensed from the steam after 2 Myr, but for some 10-100 Myr the surface stayed warm (similar to 500K), the length of time depending on how quickly the CO2 was removed into the mantle. Thereafter a lifeless Earth, heated only by the dim light of the young Sun, would have evolved into a bitterly cold ice world, The cooling trend was frequently interrupted by volcanic- or impact-induced thaws. C1 NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Zahnle, KJ (reprint author), NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. EM Kevin.J.Zahnle@nasa.gov NR 28 TC 23 Z9 24 U1 5 U2 40 PU MINERALOGICAL SOC AMER PI CHANTILLY PA 3635 CONCORDE PKWY STE 500, CHANTILLY, VA 20151-1125 USA SN 1811-5209 J9 ELEMENTS JI Elements PD AUG PY 2006 VL 2 IS 4 BP 217 EP 222 DI 10.2113/gselements.2.4.217 PG 6 WC Geochemistry & Geophysics; Mineralogy SC Geochemistry & Geophysics; Mineralogy GA 075FW UT WOS:000239870500006 ER PT J AU Rodrigues, DF Goris, J Vishnivetskaya, T Gilichinsky, D Thomashow, MF Tiedje, JM AF Rodrigues, Debora Frigi Goris, Johan Vishnivetskaya, Tatiana Gilichinsky, David Thomashow, Michael F. Tiedje, James M. TI Characterization of Exiguobacterium isolates from the Siberian permafrost. Description of Exiguobacterium sibiricum sp nov SO EXTREMOPHILES LA English DT Article DE Exiguobacterium; Exiguobacterium sibiricum sp nov; polyphasic taxonomy; Siberian permafrost ID 16S RIBOSOMAL-RNA; PHYLOGENETIC TREES; DEOXYRIBONUCLEIC ACID; NUCLEOTIDE-SEQUENCES; DNA HYBRIDIZATION; GEN-NOV; GYRB; BACTERIA; STRAINS; PCR AB Three Gram-positive bacterial strains, 7-3, 255-15 and 190-11, previously isolated from Siberian permafrost, were characterized and taxonomically classified. These microorganisms are rod-shaped, facultative aerobic, motile with peritrichous flagella and their growth ranges are from -2.5 to 40 degrees C. The chemotaxonomic markers indicated that the three strains belong to the genus Exiguobacterium. Their peptidoglycan type was A3 alpha L-Lys-Gly. The predominant menaquinone detected in all three strains was MK7. The polar lipids present were phosphatidyl-glycerol, diphosphatidyl-glycerol and phosphatidyl-ethanolamine. The major fatty acids were iso-C13:0, anteiso-C13:0, iso-C15:0, C16:0 and iso-C17:0. Phylogenetic analysis based on 16S rRNA and six diverse genes, gyrB (gyrase subunit B), rpoB (DNA-directed RNA polymerase beta subunit), recA (homologous recombination), csp (cold shock protein), hsp70 (ClassI-heat shock protein-chaperonin) and citC (isocitrate dehydrogenase), indicated that the strains were closely related to Exiguobacterium undae (DSM 14481(T)p) and Exiguobacterium antarcticum (DSM 14480(T)). On the basis of the phenotypic characteristics, phylogenetic data and DNA-DNA reassociation data, strain 190-11 was classified as E. undae, while the other two isolates, 7-3 and 255-15, comprise a novel species, for which the name Exiguobacterium sibiricum sp. nov. is proposed. C1 Michigan State Univ, NASA, Astrobiol Inst, Ctr Microbial Ecol, E Lansing, MI 48824 USA. Russian Acad Sci, Inst Physicochem & Biol Problems, Pushchino, Moscow Region, Russia. Michigan State Univ, NASA, Astrobiol Inst, DOE Plant Res Lab, E Lansing, MI 48824 USA. RP Rodrigues, DF (reprint author), Michigan State Univ, NASA, Astrobiol Inst, Ctr Microbial Ecol, 540 Plant & Soil Sci Bldg, E Lansing, MI 48824 USA. EM rodri257@msu.edu RI Rodrigues, Debora/H-4375-2012; Vishnivetskaya, Tatiana/A-4488-2008; OI Vishnivetskaya, Tatiana/0000-0002-0660-023X; Rodrigues, Debora/0000-0002-3124-1443 NR 42 TC 50 Z9 59 U1 2 U2 17 PU SPRINGER TOKYO PI TOKYO PA 3-3-13, HONGO, BUNKYO-KU, TOKYO, 113-0033, JAPAN SN 1431-0651 J9 EXTREMOPHILES JI Extremophiles PD AUG PY 2006 VL 10 IS 4 BP 285 EP 294 DI 10.1007/s00792-005-0497-5 PG 10 WC Biochemistry & Molecular Biology; Microbiology SC Biochemistry & Molecular Biology; Microbiology GA 078RB UT WOS:000240119900004 PM 16489412 ER PT J AU Jarvis, SA Spooner, DP Keung, HNLC Cao, JW Saini, S Nudd, GR AF Jarvis, Stephen A. Spooner, Daniel P. Keung, Helene N. Lim Choi Cao, Junwei Saini, Subhash Nudd, Graham R. TI Performance prediction and its use in parallel and distributed computing systems SO FUTURE GENERATION COMPUTER SYSTEMS-THE INTERNATIONAL JOURNAL OF GRID COMPUTING AND ESCIENCE LA English DT Article; Proceedings Paper CT International Workshop on Performance Modeling, Evaluation, and Optimization of Parallel and Distributed Systems CY APR 22-26, 2003 CL Nice, FRANCE DE performance prediction; resource management; grid computing ID OPTIMIZATION; SERVICE AB Performance prediction is set to play a significant role in supportive middleware that is designed to manage workload on parallel and distributed computing systems. This middleware underpins the discovery of available resources, the identification of a task's requirements and the match-making, scheduling and staging that follow. This paper documents two prediction-based middleware services that address the implications of executing a particular workload on a given set of resources. These services are based on an established performance prediction system that is employed at both the local (intra-domain) and global (multi-domain) levels to provide dynamic workload steering. These additional facilities bring about significant performance improvements, the details of which are presented with regard to system- and user-level qualities of service. The middleware has been designed for the management of resources and distributed workload across multiple administrative boundaries, a requirement that is of central importance to grid computing. (C) 2006 Elsevier B.V. All rights reserved. C1 Univ Warwick, Dept Comp Sci, Warwick CV4 7AL, England. MIT, Ctr Space Res, Cambridge, MA 02139 USA. NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Jarvis, SA (reprint author), Univ Warwick, Dept Comp Sci, Warwick CV4 7AL, England. EM stephen.jarvis@warwick.ac.uk NR 35 TC 28 Z9 29 U1 0 U2 0 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0167-739X EI 1872-7115 J9 FUTURE GENER COMP SY JI Futur. Gener. Comp. Syst. PD AUG PY 2006 VL 22 IS 7 BP 745 EP 754 DI 10.1016/j.future.2006.02.008 PG 10 WC Computer Science, Theory & Methods SC Computer Science GA 051DU UT WOS:000238141800004 ER PT J AU Peters, BT van Emmerik, REA Bloomberg, JJ AF Peters, Brian T. van Emmerik, Richard E. A. Bloomberg, Jacob J. TI Stride cycle influences on goal-directed head movements made during walking SO GAIT & POSTURE LA English DT Article DE head movement; target acquisition; locomotion; eye-head coordination; vision ID RANDOM ROTATIONS; LOCOMOTION; STABILIZATION; PLANE; GAIT AB Horizontal head movements were studied in six subjects as they made rapid horizontal gaze adjustments while walking. The aim of the present research was to determine if gait cycle events alter the head movement response to a visual target acquisition task. Gaze shifts of approximately 40 degrees were elicited by a step change in the position of a visual target from a central location to a second location in the left or right horizontal periphery. The timing of the target position change was constrained to occur at 25%, 50%, 75% and 100% of the stride cycle. The trials were randomly presented as the subjects walked on a treadmill at their preferred speed (range: 1.25-1.48 m/s, mean: 1.39 +/- 0.09 m/s). Analyses focused on the movement onset latencies of the head and eyes and on the peak velocity and saccade amplitude of the head movement response. The head and eye movement onset latencies were not affected by either the direction of the target change or the point in the gait cycle during which the target relocation occurred. However, the presence of an interaction between the gait cycle events and the direction of the visual target shift for both the amplitude and peak velocity of the head movement response indicates that the head movement responses to visual target changes can be influenced by the phase of the gait cycle during which the target relocation takes place. (C) 2005 Elsevier B.V. All rights reserved. C1 Wyle Life Sci, Neurosci Labs, Houston, TX 77058 USA. Univ Massachusetts, Dept Exercise Sci, Amherst, MA 01003 USA. NASA, Lyndon B Johnson Space Ctr, Neurosci Labs, Houston, TX 77058 USA. RP Peters, BT (reprint author), Wyle Life Sci, Neurosci Labs, 1209 Hercules Dr,Suite 120, Houston, TX 77058 USA. EM bpeters@ems.jsc.nasa.gov NR 22 TC 4 Z9 4 U1 1 U2 5 PU ELSEVIER IRELAND LTD PI CLARE PA ELSEVIER HOUSE, BROOKVALE PLAZA, EAST PARK SHANNON, CO, CLARE, 00000, IRELAND SN 0966-6362 EI 1879-2219 J9 GAIT POSTURE JI Gait Posture PD AUG PY 2006 VL 24 IS 1 BP 70 EP 76 DI 10.1016/j.gaitpost.2005.07.004 PG 7 WC Neurosciences; Orthopedics; Sport Sciences SC Neurosciences & Neurology; Orthopedics; Sport Sciences GA 066TH UT WOS:000239252500009 PM 16099655 ER PT J AU Bonifacie, M Jendrzejewski, N Agrinier, P Coleman, M Javoy, M AF Bonifacie, M. Jendrzejewski, N. Agrinier, P. Coleman, M. Javoy, M. TI The global chlorine cycle: Cl isotope constraints SO GEOCHIMICA ET COSMOCHIMICA ACTA LA English DT Meeting Abstract CT 16th Annual V M Goldschmidt Conference CY AUG-SEP -, 2006 CL Melbourne, AUSTRALIA C1 LGIS, IPGP, Paris, France. GPS, Pasadena, CA USA. JPL, Pasadena, CA USA. EM bonifaci@ipgp.jussieu.fr RI Bonifacie, Magali/A-5656-2011 NR 0 TC 1 Z9 1 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 AUG-SEP PY 2006 VL 70 IS 18 SU S BP A78 EP A78 DI 10.1016/j.gca.2006.06.260 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 096JU UT WOS:000241374200167 ER PT J AU Brandon, AD AF Brandon, A. D. TI Mantle-core interactions overview: The Os isotope perspective SO GEOCHIMICA ET COSMOCHIMICA ACTA LA English DT Meeting Abstract CT 16th Annual V M Goldschmidt Conference CY AUG-SEP -, 2006 CL Melbourne, AUSTRALIA ID OS-186-OS-187 SYSTEMATICS; KOMATIITES C1 NASA, Lyndon B Johnson Space Ctr, KR, Houston, TX 77058 USA. EM alan.d.brandon@nasa.gov NR 3 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 AUG-SEP PY 2006 VL 70 IS 18 SU S BP A63 EP A63 DI 10.1016/j.gca.2006.06.231 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 096JU UT WOS:000241374200137 ER PT J AU Debaille, V Tronnes, RG Brandon, AD Lee, CTA AF Debaille, V. Tronnes, R. G. Brandon, A. D. Lee, C. -T. A. TI Origin of the Jan Mayen hotspot: An Os-187O/Os-188 and PGE perspective SO GEOCHIMICA ET COSMOCHIMICA ACTA LA English DT Meeting Abstract CT 16th Annual V M Goldschmidt Conference CY AUG-SEP -, 2006 CL Melbourne, AUSTRALIA C1 Lunar & Planetary Inst, Houston, TX 77058 USA. Univ Oslo, Nat Hist Museum, Oslo, Norway. NASA, Johnson Space Ctr, Houston, TX USA. Rice Univ, Houston, TX 77251 USA. EM debaille@lpi.usra.edu; r.g.tronnes@nhm.uio.no; alan.d.brandon@nasa.gov; ctlee@rice.edu 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 AUG-SEP PY 2006 VL 70 IS 18 SU S BP A136 EP A136 DI 10.1016/j.gca.2006.06.289 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 096JU UT WOS:000241374200283 ER PT J AU Des Marais, DJ AF Des Marais, D. J. CA Athena Science Team TI Potential lifestyles in ancient environments of Gusev crater, Mars SO GEOCHIMICA ET COSMOCHIMICA ACTA LA English DT Meeting Abstract CT 16th Annual V M Goldschmidt Conference CY AUG-SEP -, 2006 CL Melbourne, AUSTRALIA C1 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 AUG-SEP PY 2006 VL 70 IS 18 SU S BP A139 EP A139 DI 10.1016/j.gca.2006.06.294 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 096JU UT WOS:000241374200288 ER PT J AU Flynn, GJ Keller, LP Wirick, S Jacobsen, C AF Flynn, G. J. Keller, L. P. Wirick, S. Jacobsen, C. TI Submicron-scale search for carbonate in primitive extraterrestrial materials SO GEOCHIMICA ET COSMOCHIMICA ACTA LA English DT Meeting Abstract CT 16th Annual V M Goldschmidt Conference CY AUG-SEP -, 2006 CL Melbourne, AUSTRALIA C1 SUNY Coll Plattsburgh, Plattsburgh, NY 12901 USA. NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. SUNY Stony Brook, Stony Brook, NY 11794 USA. EM george.flynn@plattsburgh.edu RI Jacobsen, Chris/E-2827-2015 OI Jacobsen, Chris/0000-0001-8562-0353 NR 3 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 AUG-SEP PY 2006 VL 70 IS 18 SU S BP A179 EP A179 DI 10.1016/j.gca.2006.06.359 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 096JU UT WOS:000241374200368 ER PT J AU Friedmann, EI Wierzchos, J Davila, A Kirschvink, JL Ascaso, C Kashai, EL Mckay, CP AF Friedmann, E. I. Wierzchos, J. Davila, A. Kirschvink, J. L. Ascaso, C. Kashai, E. L. McKay, C. P. TI Biogeochemistry on Mars, both possible and realistic: Magnetite SO GEOCHIMICA ET COSMOCHIMICA ACTA LA English DT Meeting Abstract CT 16th Annual V M Goldschmidt Conference CY AUG-SEP -, 2006 CL Melbourne, AUSTRALIA C1 NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. Univ Lleida, Lleida, Spain. CALTECH, Pasadena, CA 91125 USA. Ctr Cienc Ambient, Madrid, Spain. Zion Oil & Gas Inc, Caesarea, Israel. EM ifriedmann@mail.arc.nasa.gov; jacekw@suic-me.udl.es; fon@geophysik.uni-muenchen.de; kirschvink@caltech.edu; ascaso@ccma.csic.es; kashay@bezeqint.net; cmckay@mail.arc.nasa.gov RI Wierzchos, Jacek/F-7036-2011; Ascaso, Carmen/F-5369-2011; Davila, Alfonso/A-2198-2013 OI Wierzchos, Jacek/0000-0003-3084-3837; Ascaso, Carmen/0000-0001-9665-193X; Davila, Alfonso/0000-0002-0977-9909 NR 0 TC 0 Z9 0 U1 1 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 AUG-SEP PY 2006 VL 70 IS 18 SU S BP A185 EP A185 DI 10.1016/j.gca.2006.06.372 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 096JU UT WOS:000241374200381 ER PT J AU Golden, DC Ming, DW Morris, RV AF Golden, D. C. Ming, D. W. Morris, R. V. TI Spherulitic (c-axis) growth for terrestrial (Mauna Kea, Hawaii) and martian hematite "blueberries" SO GEOCHIMICA ET COSMOCHIMICA ACTA LA English DT Meeting Abstract CT 16th Annual V M Goldschmidt Conference CY AUG-SEP -, 2006 CL Melbourne, AUSTRALIA ID MERIDIANI-PLANUM; WATER; MARS C1 NASA, Lyndon B Johnson Space Ctr, ESCG, LE23, Houston, TX 77058 USA. Lyndon B Johnson Space Ctr, NASA, ARES, Houston, TX USA. Lyndon B Johnson Space Ctr, NASA, ARES, Houston, TX USA. EM d.c.golden@nasa.gov; douglas.w.ming@nasa.gov; richard.v.morris@nasa.gov 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 AUG-SEP PY 2006 VL 70 IS 18 SU S BP A207 EP A207 DI 10.1016/j.gca.2006.06.416 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 096JU UT WOS:000241374200424 ER PT J AU Jahnke, LL Summons, RE AF Jahnke, L. L. Summons, R. E. TI Compound-specific isotope analysis of cyanobacterial pure cultures and microbial mats: Effects of photorespiration? SO GEOCHIMICA ET COSMOCHIMICA ACTA LA English DT Meeting Abstract CT 16th Annual V M Goldschmidt Conference CY AUG-SEP -, 2006 CL Melbourne, AUSTRALIA C1 NASA, Ames Res Ctr, Exobiol Branch, Moffett Field, CA 94035 USA. Australian Geolog Survey Org, Canberra, ACT, Australia. MIT, EAPS, Cambridge, MA 02139 USA. EM linda.l.jahnke@nasa.gov; rsummons@mit.edu NR 3 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 AUG-SEP PY 2006 VL 70 IS 18 SU S BP A287 EP A287 DI 10.1016/j.gca.2006.06.583 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 096JU UT WOS:000241374200584 ER PT J AU Klingelhofer, G Morris, RV Yen, AS Ming, DW Schroder, C Rodionov, D AF Klingelhoefer, G. Morris, R. V. Yen, A. S. Ming, D. W. Schroeder, Ch. Rodionov, D. TI Mineralogy on Mars at Gusev Crater and Meridiani Planum as seen by iron Mossbauer spectroscopy SO GEOCHIMICA ET COSMOCHIMICA ACTA LA English DT Meeting Abstract CT 16th Annual V M Goldschmidt Conference CY AUG-SEP -, 2006 CL Melbourne, AUSTRALIA ID SPECTROMETER C1 Johannes Gutenberg Univ Mainz, Inst Inorgan & Analyt Chem, D-6500 Mainz, Germany. NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. CALTECH, Jet Prop Lab, Pasadena, CA USA. EM klingel@mail.uni-mainz.de; richard.v.morris@nasa.gov; douglas.w.ming@nasa.gov RI Schroder, Christian/B-3870-2009 OI Schroder, Christian/0000-0002-7935-6039 NR 6 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 AUG-SEP PY 2006 VL 70 IS 18 SU S BP A325 EP A325 DI 10.1016/j.gca.2006.06.656 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 096JU UT WOS:000241374200658 ER PT J AU McAdam, AC Zolotov, MY Mironenk, MV Leshin, LA Sharp, TG AF McAdam, A. C. Zolotov, M. Yu. Mironenko, M. V. Leshin, L. A. Sharp, T. G. TI Low pH weathering of Mars analog lithologies: Thermodynamic modeling SO GEOCHIMICA ET COSMOCHIMICA ACTA LA English DT Meeting Abstract CT 16th Annual V M Goldschmidt Conference CY AUG-SEP -, 2006 CL Melbourne, AUSTRALIA C1 Arizona State Univ, Dept Geol Sci, Tempe, AZ 85287 USA. Russian Acad Sci, Vernadsky Inst Geochem & Analyt Chem, R-119991 Moscow, Russia. NASA, Goddard Space Flight Ctr, Sci & Explorat Directorate, Greenbelt, MD 20771 USA. EM amcadam@asu.eduu RI McAdam, Amy/E-1556-2012 NR 4 TC 0 Z9 0 U1 1 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 AUG-SEP PY 2006 VL 70 IS 18 BP A406 EP A406 DI 10.1016/j.gca.2006.06.819 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 096JU UT WOS:000241374201064 ER PT J AU Merino, E Coleman, M AF Merino, E. Coleman, M. TI Weathering-made pisolites: Analogue for Martian blueberries SO GEOCHIMICA ET COSMOCHIMICA ACTA LA English DT Meeting Abstract CT 16th Annual V M Goldschmidt Conference CY AUG-SEP -, 2006 CL Melbourne, AUSTRALIA C1 Indiana Univ, Bloomington, IN 47405 USA. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. EM merino@indiana.edu; max.coleman@jpl.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 AUG-SEP PY 2006 VL 70 IS 18 SU S BP A416 EP A416 DI 10.1016/j.gca.2006.06.838 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 096JU UT WOS:000241374201084 ER PT J AU Noble, SK Keller, LP AF Noble, S. K. Keller, L. P. TI Investigating the nanoscale complexity of lunar space weathering SO GEOCHIMICA ET COSMOCHIMICA ACTA LA English DT Meeting Abstract CT 16th Annual V M Goldschmidt Conference CY AUG-SEP -, 2006 CL Melbourne, AUSTRALIA C1 NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. EM Sarah.K.Noble@nasa.gov RI Noble, Sarah/D-7614-2012 NR 0 TC 0 Z9 1 U1 0 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 AUG-SEP PY 2006 VL 70 IS 18 SU S BP A448 EP A448 DI 10.1016/j.gca.2006.06.900 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 096JU UT WOS:000241374201146 ER PT J AU Walker, RJ Ireland, T Brandon, AD AF Walker, R. J. Ireland, T. Brandon, A. D. TI The search for evidence of chemical interactions between the core and mantle SO GEOCHIMICA ET COSMOCHIMICA ACTA LA English DT Meeting Abstract CT 16th Annual V M Goldschmidt Conference CY AUG-SEP -, 2006 CL Melbourne, AUSTRALIA C1 Univ Maryland, Dept Geol, College Pk, MD 20742 USA. NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. EM rjwalker@geol.umd.edu; tireland@geol.umd.edu; alan.d.brandon@nasa.gov NR 2 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 AUG-SEP PY 2006 VL 70 IS 18 SU S BP A683 EP A683 DI 10.1016/j.gca.2006.06.1487 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 096JU UT WOS:000241374201610 ER PT J AU Zahnle, KJ AF Zahnle, K. J. TI Earth after the Moon-forming impact SO GEOCHIMICA ET COSMOCHIMICA ACTA LA English DT Meeting Abstract CT 16th Annual V M Goldschmidt Conference CY AUG-SEP -, 2006 CL Melbourne, AUSTRALIA C1 NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. EM kzahnle@mail.arc.nasa.gov NR 0 TC 4 Z9 4 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 AUG-SEP PY 2006 VL 70 IS 18 SU S BP A729 EP A729 DI 10.1016/j.gca.2006.06.1311 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 096JU UT WOS:000241374201701 ER PT J AU Henry, CD Kim, J McQuillen, J AF Henry, CD Kim, J McQuillen, J TI Dissolved gas effects on thermocapillary convection during boiling in reduced gravity environments SO HEAT AND MASS TRANSFER LA English DT Article DE microgravity; boiling; thermocapillary convection; dissolved gas ID HEAT-TRANSFER; FLOW; MICROGRAVITY; BUBBLE; FLUID AB The mechanisms by which thermocapillary convection arises during boiling of nominally pure fluids in low-g environments are currently not known. It has recently been suggested that small amounts of dissolved gas within the bulk liquid can accumulate within the vapor bubble, forming localized concentration gradients that results in a temperature gradient to form along the liquid-vapor interface that drives thermocapillary convection. This hypothesis was tested by boiling > 99.3% pure n-perfluorohexane with and without noncondensible gas in a low-g environment using a 7.0 x 7.0 mm(2) stop microheater array to measure time and space resolved heat transfer at various wall superheats. The thermocapillary convection around the primary bubble that formed in the gassy fluid was found to be much weaker than in the degassed fluid, and the primary bubble diameter was much larger in the gassy fluid due to the accumulation of noncondensible gas within the bubble. The results suggest that the accumulation of noncondensible gas in the bubble can result in temperature variations along the interface but due to the increased vapor/gas bubble size, the driving thermocapillary temperature gradient along the interface is significantly reduced and result in much weaker thermocapillary flow. The highest CHF values in a reduced gravity environment (19 W/cm(2) stop) occurred when the fluid was highly subcooled and degassed. C1 Univ Maryland, College Pk, MD 20742 USA. Intel Corp, Chandler, AZ USA. NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. RP Kim, J (reprint author), Univ Maryland, College Pk, MD 20742 USA. EM christopher.henry@intel.com; kimjh@umd.edu; John.B.McQuillen@nasa.gov NR 32 TC 25 Z9 26 U1 1 U2 12 PU SPRINGER PI NEW YORK PA 233 SPRING STREET, NEW YORK, NY 10013 USA SN 0947-7411 J9 HEAT MASS TRANSFER JI Heat Mass Transf. PD AUG PY 2006 VL 42 IS 10 BP 919 EP 928 DI 10.1007/s00231-006-0140-8 PG 10 WC Thermodynamics; Mechanics SC Thermodynamics; Mechanics GA 059OD UT WOS:000238741200007 ER PT J AU Wagner, S Dai, HX Stapleton, RA Illingsworth, ML Siochi, EJ AF Wagner, Shawn Dai, Huixiong Stapleton, Russell A. Illingsworth, Marvin L. Siochi, Emilie J. TI Pendent polyimides using mellitic acid dianhydride. 1. An atomic oxygen-resistant, pendent 4,4 ' ODA/PMDA/MADA co-polyimide containing zirconium SO HIGH PERFORMANCE POLYMERS LA English DT Article DE mellitic acid dianhydride; benzenehexacarboxylic acid dianhydride; polyimide; pendent; atomic oxygen; zirconium ID LOW-EARTH-ORBIT; POLYMERS; COMPLEX; PLASMA; FILMS AB The goal of this research is to increase the metal-organic concentration in Kapton-like polyimides (PIs) to achieve increased atomic oxygen (AO) resistance while retaining desirable film properties. Co-polyamic acid (PAA) precursors were prepared using a novel polymer building block, mellitic acid dianhydride (MADA), to provide sites for pendent group attachment. Attachment of an amino group-functionalized zirconium complex to the co-PAA precursors was facilitated by a stoichiometric amount of dicyclohexylcarbodiimide. The viscous solutions which resulted were characterized by thin layer chromatography (TLC), viscosity, and gel permeation chromatography (GPC), or treated with excess poor solvent to precipitate powder samples, or cast onto glass slides and heated to produce imidized films. Powder samples were dissolved in deuterated solvent for proton nuclear magnetic resonance analysis, or characterized by thermogravimetric analysis and differential scanning calorimetry. Film samples were characterized by Fourier transform infrared and by scanning electron microscopy (SEM) before and after exposure to atomic oxygen in a plasma asher. The spectroscopic data are consistent with the expected amic acid and imide, pendent and non-pendent structures. TLC, viscosity and GPC results confirm the polymeric nature of the pendent and non-pendent co-PAA precursors, with inherent viscosities (eta(o)) of 0.76 and 0.65 and weight average molecular weights (M-w) estimated to be 61 000 and 138 000 Dalton,. respectively. As expected, visual and SEM inspections of pendent and non-pendent co-PI films reveal extensive surface roughening upon exposure to AO, with the former developing a white surface layer known from model compound studies to be predominantly zirconium dioxide. Additional reports describing the effects of polymer structure and pendent group concentration on film properties and AO resistance are in preparation. C1 Rochester Inst Technol, Dept Chem, Rochester, NY 14623 USA. NASA, Langley Res Ctr, Hampton, VA 23681 USA. RP Siochi, EJ (reprint author), Rochester Inst Technol, Dept Chem, Rochester, NY 14623 USA. EM mlisch@rit.edu NR 24 TC 15 Z9 17 U1 1 U2 13 PU SAGE PUBLICATIONS LTD PI LONDON PA 1 OLIVERS YARD, 55 CITY ROAD, LONDON EC1Y 1SP, ENGLAND SN 0954-0083 J9 HIGH PERFORM POLYM JI High Perform. Polym. PD AUG PY 2006 VL 18 IS 4 BP 399 EP 419 DI 10.1177/0954008305055012 PG 21 WC Polymer Science SC Polymer Science GA 066PZ UT WOS:000239243900001 ER PT J AU Hawkins, BP Hinkley, JA Pater, RH Moore, J AF Hawkins, Brian P. Hinkley, Jeffrey A. Pater, Ruth H. Moore, Joanne TI Stretch-orientation of LaRC (TM) RP50 polyimide film SO HIGH PERFORMANCE POLYMERS LA English DT Article DE orientation; thermosetting; polyimide; addition polyimide; biaxial; film ID IMIDIZATION AB An addition-curable poly(amic acid) film was subjected to various thermal pretreatments and then to uniaxial or biaxial drawing. Hot-stretching to 300% of the initial length produced better than twofold increases in tensile modulus and strength of partially-cured films. Most of the improvement was maintained upon completion of the curing at constant length. C1 NASA, Langley Res Ctr, Hampton, VA 23681 USA. Univ Texas, Dept Aerosp Engn & Engn Mech, Austin, TX 78712 USA. Univ Virginia, Dept Chem, Charlottesville, VA 22903 USA. RP Pater, RH (reprint author), NASA, Langley Res Ctr, Hampton, VA 23681 USA. EM Ruth.H.Pater@nasa.gov NR 13 TC 2 Z9 2 U1 1 U2 2 PU SAGE PUBLICATIONS LTD PI LONDON PA 1 OLIVERS YARD, 55 CITY ROAD, LONDON EC1Y 1SP, ENGLAND SN 0954-0083 J9 HIGH PERFORM POLYM JI High Perform. Polym. PD AUG PY 2006 VL 18 IS 4 BP 469 EP 478 DI 10.1177/0954008306066334 PG 10 WC Polymer Science SC Polymer Science GA 066PZ UT WOS:000239243900005 ER PT J AU Ghose, S Watson, KA Working, DC Siochi, EJ Connell, JW Criss, JM AF Ghose, Sayata Watson, Kent A. Working, Dennis C. Siochi, Emilie J. Connell, John W. Criss, Jim M. TI Fabrication and characterization of high temperature resin/carbon nanofiber composites SO HIGH PERFORMANCE POLYMERS LA English DT Article DE resins; carbon nanofibers; scanning electron microscopy; electrical properties; thermal conductivity ID BALL-MILLED CARBON; POLYMER-MATRIX; NANOTUBES; MORPHOLOGY; FIBERS AB Multifunctional composites present a route to structural weight reduction. Nanoparticles such as carbon nanofibers (CNF) provide a compromise as a lower cost nanosize reinforcement that yields a desirable combination of properties. Blends of PETI-330 and CNFs were prepared and characterized to investigate the potential of CNF composites as a high-performance structural medium. Dry mixing techniques were employed and the effect of CNF loading level on melt viscosity was determined. The resulting powders were characterized for degree of mixing, thermal and rheological properties. Based on the characterization results, samples containing 30 and 40 wt.% CNF were scaled up to approximately 300 g and used to fabricate moldings 10.2 cm x 15.2 cm x 0.32 cm thick. The moldings were fabricated by injecting the mixtures at 260-280 degrees C into a stainless steel tool followed by curing for 1 h at 371 degrees C. The tool was designed to impart high shear during the injection process in an attempt to achieve some alignment of CNFs in the flow direction. Moldings were obtained that were subsequently characterized for thermal, mechanical and electrical properties. The degree of dispersion and alignment of CNFs were investigated using high-resolution scanning electron microscopy. The preparation and preliminary characterization of PETI-330/CNF composites are discussed. C1 NASA, Langley Res Ctr, Hampton, VA 23681 USA. NASA, LaRC, Hampton, VA 23681 USA. Natl Inst Aerosp, Hampton, VA 23666 USA. M&P Technol Inc, Marietta, GA 30068 USA. RP Connell, JW (reprint author), NASA, Langley Res Ctr, Hampton, VA 23681 USA. EM John.W.Connell@nasa.gov NR 26 TC 16 Z9 16 U1 3 U2 14 PU SAGE PUBLICATIONS LTD PI LONDON PA 1 OLIVERS YARD, 55 CITY ROAD, LONDON EC1Y 1SP, ENGLAND SN 0954-0083 J9 HIGH PERFORM POLYM JI High Perform. Polym. PD AUG PY 2006 VL 18 IS 4 BP 527 EP 544 DI 10.1177/0954008306066538 PG 18 WC Polymer Science SC Polymer Science GA 066PZ UT WOS:000239243900009 ER PT J AU Fast, K Kostiuk, T Hewagama, T A'Hearn, MF Livengood, TA Lebonnois, S Lefevre, F AF Fast, Kelly Kostiuk, Theodor Hewagama, Tilak A'Hearn, Michael F. Livengood, Timothy A. Lebonnois, Sebastien Lefevre, Franck TI Ozone abundance on Mars from infrared heterodyne spectra II. Validating photochemical models SO ICARUS LA English DT Article DE Mars; atmosphere; photochemistry; infrared observations; spectroscopy; abundances; atmospheres ID MARTIAN ATMOSPHERE; WATER-VAPOR; GLOBAL DISTRIBUTION; SEASONAL-VARIATION; STABILITY; APHELION; SPECTROMETER; DENSITY AB Ozone is an important observable tracer of martian photochemistry. including odd hydrogen (HO(x)) species important to the chemistry and stability of the martian atmosphere. Infrared heterodyne spectroscopy with spectral resolution >= 10(6) provides the only ground-based direct access to ozone absorption features in the martian atmosphere. Ozone abundances were measured with the Goddard Infrared Heterodyne Spectrometer and the Heterodyne Instrument for Planetary Wind and Composition at the NASA Infrared Telescope Facility on Mauna Kea, Hawai'i. Retrieved total ozone column abundances from various latitudes and orbital positions (L(S) = 40 degrees, 74 degrees, 102 degrees, 115 degrees, 202 degrees, 208 degrees, 291 degrees) are compared to those predicted by the first three-dimensional gas phase photochemical model of the martian atmosphere [Lefevre. F., Lebonnois, S., Montmessin, F., Forget, F., 2004. J. Geophys. Res. 109, doi: 10.1029/2004JE002268. E07004]. Observed and modeled ozone abundances show good agreement at all latitudes at perihelion orbital positions (LS = 202 degrees, 208 degrees, 291 degrees). Observed low-latitude ozone abundances are significantly higher than those predicted by the model at aphelion orbital positions (L(S) = 40 degrees, 74 degrees, 115 degrees). Heterogeneous loss of odd hydrogen onto water ice cloud particles would explain the discrepancy, as clouds are observed at low latitudes around aphelion on Mars. (c) 2006 Elsevier Inc. All rights reserved. C1 NASA, Goddard Space Flight Ctr, Planetary Syst Lab, Greenbelt, MD 20771 USA. Univ Maryland, Dept Astron, College Pk, MD 20742 USA. USRA, Natl Ctr Earth & Space Sci Educ, Washington, DC 20036 USA. Inst Pierre Simon Laplace, Meteorol Dynam Lab, F-75252 Paris 05, France. CSIC, Inst Astrofis Andalucia, E-18080 Granada, Spain. RP Fast, K (reprint author), NASA, Goddard Space Flight Ctr, Planetary Syst Lab, Code 693, Greenbelt, MD 20771 USA. EM kelly.e.fast@nasa.gov RI Livengood, Timothy/C-8512-2012; Kostiuk, Theodor/A-3077-2014; Hewagama, T/C-8488-2012 NR 34 TC 16 Z9 16 U1 0 U2 2 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 J9 ICARUS JI Icarus PD AUG PY 2006 VL 183 IS 2 BP 396 EP 402 DI 10.1016/j.icarus.2006.03.012 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 067WB UT WOS:000239332200011 ER PT J AU Ostro, SJ West, RD Janssen, MA Lorenz, RD Zebker, HA Black, GJ Lunine, JI Wye, LC Lopes, RM Wall, SD Elachi, C Roth, L Hensley, S Kelleher, K Hamilton, GA Gim, Y Anderson, YZ Boehmer, RA Johnson, WTK AF Ostro, Steven J. West, Richard D. Janssen, Michael A. Lorenz, Ralph D. Zebker, Howard A. Black, Gregory J. Lunine, Jonathan I. Wye, Lauren C. Lopes, Rosaly M. Wall, Stephen D. Elachi, Charles Roth, Laci Hensley, Scott Kelleher, Kathleen Hamilton, Gary A. Gim, Yonggyu Anderson, Yanhua Z. Boehmer, Rudy A. Johnson, William T. K. CA Cassini RADAR Team TI Cassini RADAR observations of Enceladus, Tethys, Dione, Rhea, Iapetus, Hyperion, and Phoebe SO ICARUS LA English DT Article DE Satellites of Saturn; surfaces; satellite; radar ID ICY GALILEAN SATELLITES; DIELECTRIC-PROPERTIES; MAINBELT ASTEROIDS; DARK SIDE; TITAN; SURFACE; VENUS; ARECIBO; THOLINS; EUROPA AB Cassini 2.2-cm radar and radiometric observations of seven of Saturn's icy satellites yield properties that apparently are dominated by subsurface volume scattering and are similar to those of the icy Galilean satellites. Average radar albedos decrease in the order Enceladus/Tethys, Hyperion, Rhea, Dione, lapetus, and Phoebe. This sequence most likely corresponds to increasing contamination of near-surface water ice, which is intrinsically very transparent at radio wavelengths. Plausible candidates for contaminants include ammonia, silicates, metallic oxides, and polar organics (ranging from nitriles like HCN to complex tholins). There is correlation of our targets' radar and optical albedos, probably due to variations in the concentration of optically dark contaminants in near-surface water ice and the resulting variable attenuation of the high-order multiple scattering responsible for high radar albedos. Our highest radar albedos, for Enceladus and Tethys, probably require that at least the uppermost one to several decimeters of the surface be extremely clean water ice regolith that is structurally complex (i.e., mature) enough for there to be high-order multiple scattering within it. At the other extreme, Phoebe has an asteroidal radar reflectivity that may be due to a combination of single and volume scattering. Iapetus' 2.2-cm radar albedo is dramatically higher on the optically bright trailing side than the optically dark leading side, whereas 13-cm results reported by Black et al. [Black, G.J., Campbell, D.B., Carter, L.M., Ostro, S.J., 2004. Science 304, 553] show hardly any hemispheric asymmetry and give a mean radar reflectivity several times lower than the reflectivity measured at 2.2 cm. These Iapetus results are understandable if ammonia is much less abundant on both sides within the upper one to several decimeters than at greater depths, and if the leading side's optically dark contaminant is present to depths of at least one to several decimeters. As argued by Lanzerotti et al. [Lanzerotti, L.J., Brown, W.L., Marcantonio, K.J., Johnson, R.E., 1984. Nature 312, 139-140], a combination of ion erosion and micrometeoroid gardening may have depleted ammonia from the surfaces of Saturn's icy satellites. Given the hypersensitivity of water ice's absorption length to ammonia concentration, an increase in ammonia with depth could allow efficient 2.2-cm scattering from within the top one to several decimeters while attenuating 13-cm echoes, which would require a six-fold thicker scattering layer. If so, we would expect each of the icy satellites' average radar albedos to be higher at 2.2 cm than at 13 cm, as is the case so far with Rhea [Black, G., Campbell, D., 2004. Bull. Am. Astron. Soc. 36, 1123] as well as Iapetus. (c) 2006 Elsevier Inc. All rights reserved. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA. Stanford Univ, Dept Elect Engn, Stanford, CA 94305 USA. Univ Virginia, Dept Astron, Charlottesville, VA 22903 USA. INAF, IFSI, ARTOV, I-00133 Rome, Italy. RP Ostro, SJ (reprint author), CALTECH, Jet Prop Lab, Mail Stop 300-233,4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM ostro@reason.jpl.nasa.gov RI Lorenz, Ralph/B-8759-2016; Lopes, Rosaly/D-1608-2016 OI Lorenz, Ralph/0000-0001-8528-4644; Lopes, Rosaly/0000-0002-7928-3167 NR 65 TC 48 Z9 48 U1 1 U2 6 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 J9 ICARUS JI Icarus PD AUG PY 2006 VL 183 IS 2 BP 479 EP 490 DI 10.1016/j.icarus.2006.02.019 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 067WB UT WOS:000239332200018 ER PT J AU U-Yen, K Wollack, EJ Doiron, T Papapolymerou, J Laskar, J AF U-Yen, Kongpop Wollack, Edward J. Doiron, Terence Papapolymerou, John Laskar, Joy TI A bandpass filter design using half-wavelength stepped impedance resonators with internal couplings SO IEEE MICROWAVE AND WIRELESS COMPONENTS LETTERS LA English DT Article DE bandpass filters (BPFs); microstrip; transmission line resonators AB We propose a new type of microstrip half-wavelength (lambda/2) stepped impedance resonator (SIR) for use in bandpass filter (BPF) designs. This lambda/2 SIR has an internal coupling section that can be used to generate a coupling coefficient in the filter design in addition to couplings between. SIRs. It also contains additional stepped impedance lines that shift and suppress the lowest even-mode resonance frequencies to more than what can be achieved by conventional lambda/2 SIRs. Moreover, a transmission zero is generated close to its fundamental resonance frequency (f(0)) which can be used in definition of the filter response. A fourth-order microstrip BPF with 10% bandwidth was constructed using two of the proposed lambda/2 SIRs with a stepped impedance ratio A of 0.528. The experimental result shows that the filter can achieve low in-band loss and out-of-band attenuation of 52.6 dB up to 3 f(0). The lowest spurious resonance frequency is shifted to 3 f(0) as opposed to 2.5 f(0) in conventional lambda/2 SIRs with the same R value. C1 NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Georgia Inst Technol, Sch Elect & Comp Engn, Atlanta, GA 30332 USA. RP U-Yen, K (reprint author), NASA, Goddard Space Flight Ctr, Code 661, Greenbelt, MD 20771 USA. EM kuyen@pop500.gsfc.nasa.gov; papapol@ece.gatech.edu RI Wollack, Edward/D-4467-2012 OI Wollack, Edward/0000-0002-7567-4451 NR 4 TC 2 Z9 2 U1 0 U2 2 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855 USA SN 1531-1309 J9 IEEE MICROW WIREL CO JI IEEE Microw. Wirel. Compon. Lett. PD AUG PY 2006 VL 16 IS 8 BP 443 EP 445 DI 10.1109/LMWC.2006.879494 PG 3 WC Engineering, Electrical & Electronic SC Engineering GA 068FA UT WOS:000239356700003 ER PT J AU Simon, MK AF Simon, Marvin K. TI Comments on "infinite-series representations associated with the bivariate Rician distribution and their applications" SO IEEE TRANSACTIONS ON COMMUNICATIONS LA English DT Editorial Material C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Simon, MK (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM marvin.k.simon@jpl.nasa.gov NR 5 TC 15 Z9 15 U1 1 U2 3 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855 USA SN 0090-6778 J9 IEEE T COMMUN JI IEEE Trans. Commun. PD AUG PY 2006 VL 54 IS 8 BP 1511 EP 1512 DI 10.1109/TCOMM.2006.878821 PG 2 WC Engineering, Electrical & Electronic; Telecommunications SC Engineering; Telecommunications GA 076BY UT WOS:000239933200019 ER PT J AU Franceschetti, G Callahan, PS Iodice, A Riccio, D Wall, SD AF Franceschetti, Giorgio Callahan, Philip S. Iodice, Antonio Riccio, Daniele Wall, Stephen D. TI Titan, fractals, and filtering of Cassini altimeter data SO IEEE TRANSACTIONS ON GEOSCIENCE AND REMOTE SENSING LA English DT Article DE extraterrestrial exploration; filtering; fractals; radar altimetry ID SURFACES AB Fractal behavior of one Titan profile acquired by the Cassini altimeter during its first flyby is demonstrated and quantitatively analyzed. The inadequacy of popular nonfractal models to represent scale-dependent behavior is also discussed. Our results lead to the conjecture that a proper geometrical model of the Titan surface is provided by the fractional Brownian motion stochastic process and that the particular acquired profile has a fractal dimension of about 2.4. In addition, use of the developed statistical model allows the design of model-based filters for a significant improvement of the measurement accuracy, at the expense of the horizontal resolution. C1 Univ Naples Federico II, Dept Elect & Telecommun Engn, I-80125 Naples, Italy. Univ Calif Los Angeles, Los Angeles, CA 95147 USA. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Franceschetti, G (reprint author), Univ Naples Federico II, Dept Elect & Telecommun Engn, I-80125 Naples, Italy. EM gfrance@unina.it; philip.s.callahan@jpl.nasa.gov; iodice@unina.it; daniele.riccio@unina.it; stephen.d.wall@jpl.nasa.gov OI Iodice, Antonio/0000-0001-6173-3601 NR 13 TC 4 Z9 4 U1 0 U2 2 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855 USA SN 0196-2892 J9 IEEE T GEOSCI REMOTE JI IEEE Trans. Geosci. Remote Sensing PD AUG PY 2006 VL 44 IS 8 BP 2055 EP 2062 DI 10.1109/TGRS.2006.872152 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 068WA UT WOS:000239404000004 ER PT J AU Tedesco, M Kim, EJ AF Tedesco, Marco Kim, Edward J. TI Retrieval of dry-snow parameters from microwave radiometric data using a dense-medium model and genetic algorithms SO IEEE TRANSACTIONS ON GEOSCIENCE AND REMOTE SENSING LA English DT Article DE dense-medium radiative transfer theory (DMRT); genetic algorithms (GAs); microwave remote sensing; snow ID WATER EQUIVALENT; NEURAL-NETWORK; DEPTH AB A numerical technique based on genetic algorithms (GAs) is used to invert the equations of an electromagnetic model based on dense-medium radiative transfer theory (DMRT) to retrieve snow depth, mean grain size, and fractional volume from microwave brightness temperatures. In order to study the sensitivity of the GA to its parameters, the technique is initially tested on simulated microwave data with and without adding a random noise. A configuration of GA parameters is selected and used for the retrieval of snow parameters from both ground-based observations and brightness temperatures recorded by the Advanced Microwave Scanning Radiometer-EOS (AMSR-E). Retrieved snow parameters are then compared with those measured on ground. Although more investigation is required, results suggest that the proposed technique is able to retrieve snow parameters with good accuracy. C1 Univ Maryland Baltimore Cty, Goddard Earth Sci Technol Ctr, Baltimore, MD 21228 USA. NASA, Goddard Space Flight Ctr, Lab Hydrospher & Biosphere Proc, Greenbelt, MD 20771 USA. RP Tedesco, M (reprint author), Univ Maryland Baltimore Cty, Goddard Earth Sci Technol Ctr, Baltimore, MD 21228 USA. EM mtedesco@umbc.edu RI Tedesco, Marco/F-7986-2015 NR 26 TC 14 Z9 14 U1 0 U2 7 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855 USA SN 0196-2892 J9 IEEE T GEOSCI REMOTE JI IEEE Trans. Geosci. Remote Sensing PD AUG PY 2006 VL 44 IS 8 BP 2143 EP 2151 DI 10.1109/TGRS.2006.872087 PG 9 WC Geochemistry & Geophysics; Engineering, Electrical & Electronic; Remote Sensing; Imaging Science & Photographic Technology SC Geochemistry & Geophysics; Engineering; Remote Sensing; Imaging Science & Photographic Technology GA 068WA UT WOS:000239404000013 ER PT J AU Shokr, M Markus, T AF Shokr, Mohammed Markus, Thorsten TI Comparison of NASA Team2 and AES-York ice concentration algorithms against operational ice charts from the Canadian ice service SO IEEE TRANSACTIONS ON GEOSCIENCE AND REMOTE SENSING LA English DT Article DE Atmospheric Environment Service (AES)-York algorithm; data fusion; Enhanced NASA Team (NT2) algorithm; ice retrieval algorithms; operational ice monitoring; passive microwave for ice; Radarsat; sea ice concentration ID RETRIEVALS AB Ice concentration retrieved from spaceborne passive-microwave observations is a prime input to operational sea-ice-monitoring programs, numerical weather prediction models, and global climate models. Atmospheric Environment Service (AES)-York and the Enhanced National Aeronautics and Space Administration Team (NT2) are two algorithms that calculate ice concentration from Special Sensor Microwave/Imager observations. This paper furnishes a comparison between ice concentrations (total, thin, and thick types) output from NT2 and AES-York algorithms against the corresponding estimates from the operational analysis of Radarsat images in the Canadian Ice Service (CIS). A new data fusion technique, which incorporates the actual sensor's footprint, was developed to facilitate this study. Results have shown that the NT2 and AES-York algorithms underestimate total ice concentration by 18.35% and 9.66% concentration counts on average, with 16.8% and 15.35% standard deviation, respectively. However, the retrieved concentrations of thin and thick ice are in much more discrepancy with the operational CIS estimates when either one of these two types dominates the viewing area. This is more likely to occur when the total ice concentration approaches 100%. If thin and thick ice types coexist in comparable concentrations, the algorithms' estimates agree with CIS's estimates. In terms of ice concentration retrieval, thin ice is more problematic than thick ice. The concept of using a single tie point to represent a thin ice surface is not realistic and provides the largest error source for retrieval accuracy. While AES-York provides total ice concentration in slightly more agreement with CIS's estimates, NT2 provides better agreement in retrieving thin and thick ice concentrations. C1 Environm Canada, Meteorol Serv Canada, Toronto, ON M3H 5T4, Canada. NASA, Goddard Space Flight Ctr, Hydrospher & Biospher Sci Lab, Greenbelt, MD 20771 USA. RP Shokr, M (reprint author), Environm Canada, Meteorol Serv Canada, Toronto, ON M3H 5T4, Canada. EM mohammed.shokr@ec.ge.ca RI Markus, Thorsten/D-5365-2012 NR 26 TC 13 Z9 13 U1 0 U2 5 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855 USA SN 0196-2892 J9 IEEE T GEOSCI REMOTE JI IEEE Trans. Geosci. Remote Sensing PD AUG PY 2006 VL 44 IS 8 BP 2164 EP 2175 DI 10.1109/TGRS.2006.872077 PG 12 WC Geochemistry & Geophysics; Engineering, Electrical & Electronic; Remote Sensing; Imaging Science & Photographic Technology SC Geochemistry & Geophysics; Engineering; Remote Sensing; Imaging Science & Photographic Technology GA 068WA UT WOS:000239404000015 ER PT J AU Xiong, X Che, N Barnes, WL AF Xiong, X. Che, N. Barnes, W. L. TI Terra MODIS on-orbit spectral characterization and performance SO IEEE TRANSACTIONS ON GEOSCIENCE AND REMOTE SENSING LA English DT Article DE calibration; instrument; remote sensing ID CALIBRATION ASSEMBLY SRCA; SPATIAL CHARACTERISTICS; IMAGING SPECTROMETER; INSTRUMENT; SATELLITE AB The Moderate Resolution Imaging Spectroradiometer (MODIS) protoflight model onboard the National Aeronautics and Space Administration's Earth Observing System Terra spacecraft has been in operation for over five years since its launch in December 1999. It makes measurements using 36 spectral bands with wavelengths from 0.41 to 14.5 mu m. Bands 1-19 and 26 with wavelengths below 2.2 mu m, the reflective solar bands (RSBs), collect daytime reflected solar radiance at three nadir spatial resolutions: 0.25 km (bands 1-2), 0.5 km (bands 3-7), and 1 km (bands 8-19 and 26). Bands 20-25 and 27-36, the thermal emissive bands, collect both daytime and nighttime thermal emissions, at 1-km nadir spatial resolution. The MODIS spectral characterization was performed prelaunch at the system level. One of the MODIS onboard calibrators, the Spectroradiometric Calibration Assembly (SRCA), was designed to perform on-orbit spectral characterization of the MODIS RSB. This paper provides a brief overview of MODIS prelaunch spectral characterization, but focuses primarily on the algorithms and results of using the SRCA for on-orbit spectral characterization. Discussions are provided on the RSB center wavelength measurements and their relative spectral response retrievals, comparisons of on-orbit results with those from prelaunch measurements, and the dependence of center wavelength shifts on instrument temperature. For Terra MODIS, the center wavelength shifts over the past five years are less than 0.5 nm for most RSBs, indicating excellent stability of the instrument's spectral characteristics. Similar spectral performance has also been obtained from the Aqua MODIS (launched in May 2002) SRCA measurements. C1 NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Sci Syst & Applicat Inc, Lanham, MD 20706 USA. Univ Maryland Baltimore Cty, Baltimore, MD 21250 USA. RP Xiong, X (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. EM xioaxiong.xiong.1@gsfc.nasa.gov; nianzeng_che@ssaihq.com; wbarnes@neptune.gsfc.nasa.gov NR 20 TC 58 Z9 59 U1 2 U2 5 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855 USA SN 0196-2892 J9 IEEE T GEOSCI REMOTE JI IEEE Trans. Geosci. Remote Sensing PD AUG PY 2006 VL 44 IS 8 BP 2198 EP 2206 DI 10.1109/TGRS.2006.872083 PG 9 WC Geochemistry & Geophysics; Engineering, Electrical & Electronic; Remote Sensing; Imaging Science & Photographic Technology SC Geochemistry & Geophysics; Engineering; Remote Sensing; Imaging Science & Photographic Technology GA 068WA UT WOS:000239404000018 ER PT J AU Gao, F Masek, J Schwaller, M Hall, F AF Gao, Feng Masek, Jeff Schwaller, Matt Hall, Forrest TI On the blending of the Landsat and MODIS surface reflectance: Predicting daily Landsat surface reflectance SO IEEE TRANSACTIONS ON GEOSCIENCE AND REMOTE SENSING LA English DT Article DE data fusion; image enhancement; image processing; Landsat; Moderate Resolution Imaging Spectroradiometer (MODIS); remote sensing; surface reflectance ID WAVELET DECOMPOSITION; THEMATIC MAPPER; DATA SET AB The 16-day revisit cycle of Landsat has long limited its use for studying global biophysical processes, which evolve rapidly during the growing season. In cloudy areas of the Earth, the problem is compounded, and researchers are fortunate to get two to three clear images per year. At the same time, the coarse resolution of sensors such as the Advanced Very High Resolution Radiometer and Moderate Resolution Imaging Spectroradiometer (MODIS) limits the sensors' ability to quantify biophysical processes in heterogeneous landscapes. In this paper, the authors present a new spatial and temporal adaptive reflectance fusion model (STARFM) algorithm to blend Landsat and MODIS surface reflectance. Using this approach, high-frequency temporal information from MODIS and high-resolution spatial information from Landsat can be blended for applications that require high resolution in both time and space. The MODIS daily 500-m surface reflectance and the 16-day repeat cycle Landsat Enhanced Thematic Mapper Plus (ETM+) 30-m surface reflectance are used to produce a synthetic "daily" surface reflectance product at ETM+ spatial resolution. The authors present results both with simulated (model) data and actual Landsat/MODIS acquisitions. In general, the STARFM accurately predicts surface reflectance at an effective resolution close to that of the ETM+. However, the performance depends on the characteristic patch size of the landscape and degrades somewhat when used on extremely heterogeneous fine-grained landscapes. C1 Earth Resources Technol Inc, Jessup, MD 20794 USA. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Gao, F (reprint author), Earth Resources Technol Inc, Jessup, MD 20794 USA. EM Feng.Gao@nasa.gov RI Gao, Feng/F-3944-2010; Masek, Jeffrey/D-7673-2012 NR 9 TC 341 Z9 382 U1 20 U2 135 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855 USA SN 0196-2892 J9 IEEE T GEOSCI REMOTE JI IEEE Trans. Geosci. Remote Sensing PD AUG PY 2006 VL 44 IS 8 BP 2207 EP 2218 DI 10.1109/TGRS.2006.872081 PG 12 WC Geochemistry & Geophysics; Engineering, Electrical & Electronic; Remote Sensing; Imaging Science & Photographic Technology SC Geochemistry & Geophysics; Engineering; Remote Sensing; Imaging Science & Photographic Technology GA 068WA UT WOS:000239404000019 ER PT J AU Salvatori, G Suh, KI Ansari, RR Rovati, L AF Salvatori, Giorgia Suh, K. I. Ansari, R. R. Rovati, Luigi TI Instrumentation and calibration protocol for a continuous wave near infrared hemoximeter SO IEEE TRANSACTIONS ON INSTRUMENTATION AND MEASUREMENT LA English DT Article; Proceedings Paper CT 22nd IEEE Instrumentation and Measurement Technology Conference CY MAY 17-19, 2005 CL Ottawa, CANADA SP IEEE Instrumentat & Measurement Soc DE attenuation measurements; biomedical measurements; calibration; scattering; spectroscopy ID LIGHT; SPECTROSCOPY; SCATTERING; DIFFUSION; TISSUES; NM AB Quantification of hemoglobin content in vivo using continuous wave (CW) near infrared spectroscopy requires an accurate calibration of the measuring system. The authors introduce a recently developed instrument and focus their attention on the calibration issue, proposing a calibration procedure specifically designed for their system, but which can be easily generalized for other CW near-infrared systems. In the paper, the most important calibration procedures and the results obtained are discussed in detail. C1 Univ Modena, Dept Informat Engn, I-41100 Modena, Italy. Ohio Aerosp Inst, Cleveland, OH 44142 USA. NASA, Vis Res Lab, Glenn Res Ctr, Cleveland, OH 44135 USA. RP Salvatori, G (reprint author), Univ Modena, Dept Informat Engn, I-41100 Modena, Italy. EM salvatori.giorgia@unimore.it; Kwang.I.Suh@grc.nasa.gov; Rafat.R.Ansari@grc.nasa.gov; rovati.luigi@unimore.it RI Rovati, Luigi/K-3445-2015 OI Rovati, Luigi/0000-0002-1743-3043 NR 17 TC 10 Z9 10 U1 0 U2 4 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855 USA SN 0018-9456 J9 IEEE T INSTRUM MEAS JI IEEE Trans. Instrum. Meas. PD AUG PY 2006 VL 55 IS 4 BP 1368 EP 1376 DI 10.1109/TIM.2006.877722 PG 9 WC Engineering, Electrical & Electronic; Instruments & Instrumentation SC Engineering; Instruments & Instrumentation GA 065UI UT WOS:000239184900045 ER PT J AU Johnston, AH Rax, BG AF Johnston, Allan H. Rax, Bernard G. TI Testing and qualifying linear integrated circuits for radiation degradation in space SO IEEE TRANSACTIONS ON NUCLEAR SCIENCE LA English DT Article; Proceedings Paper CT 8th European Conference on Radiation and its Effects on Components and Systems CY SEP 19-23, 2005 CL Cap d Agde, FRANCE SP Univ Montpellier II DE hardness assurance; linear integrated circuits; radiation testing; space radiation ID LOW-DOSE-RATE; VOLTAGE REGULATOR; PROTON-RADIATION; RATE SENSITIVITY; BIPOLAR-DEVICES; DAMAGE AB This paper discusses mechanisms and circuit-related factors that affect the degradation of linear integrated circuits from radiation in space. For some circuits there is sufficient degradation to affect performance at total dose levels below 4 krad(Si) because the circuit design techniques require higher gain for the pop transistors that are the most sensitive to radiation. Qualification methods are recommended that include displacement damage as well as ionization damage. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Johnston, AH (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM allan.h.johnston@jpl.nasa.gov; bernad.g.rax@jpl.nasa.gov NR 18 TC 11 Z9 11 U1 0 U2 4 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855 USA SN 0018-9499 J9 IEEE T NUCL SCI JI IEEE Trans. Nucl. Sci. PD AUG PY 2006 VL 53 IS 4 BP 1779 EP 1786 DI 10.1109/TNS.2006.878291 PN 1 PG 8 WC Engineering, Electrical & Electronic; Nuclear Science & Technology SC Engineering; Nuclear Science & Technology GA 080JD UT WOS:000240242800006 ER PT J AU McMorrow, D Buchner, S Baze, M Bartholet, B Katz, R O'Bryan, M Poivey, C LaBel, KA Ladbury, R Maher, M Sexton, FW AF McMorrow, Dale Buchner, Stephen Baze, Mark Bartholet, Bill Katz, Richard O'Bryan, Martha Poivey, Christian LaBel, Kenneth A. Ladbury, Ray Maher, Mike Sexton, Fred W. TI Laser-Induced latchup screening and mitigation in CMOS devices SO IEEE TRANSACTIONS ON NUCLEAR SCIENCE LA English DT Article; Proceedings Paper CT 8th European Conference on Radiation and its Effects on Components and Systems CY SEP 19-23, 2005 CL Cap d Agde, FRANCE SP Univ Montpellier II DE CMOS; laser; latchup; micro-latchup; picosecond; single-event effects; single-event latchup (SEL) ID SINGLE-EVENT UPSET; 2-PHOTON ABSORPTION; PULSED-LASER; THROUGH-WAFER AB The application of the pulsed laser approach for identifying latch-up sensitive regions in CMOS circuitry is described. The utility of this approach for preliminary latchup screening of both COTS and space-qualified parts for applications in radiation environments is described. An application of hardening-by-design principles in which a space-qualified CMOS product is modified, based on the pulsed laser results, to be latchup immune, is presented in detail. The design modifications are described. C1 USN, Res Lab, Washington, DC 20375 USA. NASA, Goddard Space Flight Ctr, QSS Grp Inc, Greenbelt, MD 20771 USA. Boeing Co, Seattle, WA 98124 USA. NASA, Off Log Design, Greenbelt, MD USA. NASA, MEI Technol, Greenbelt, MD 20771 USA. Natl Semicond Corp, Portland, ME 04106 USA. Sandia Natl Labs, Albuquerque, NM 87185 USA. RP McMorrow, D (reprint author), USN, Res Lab, Washington, DC 20375 USA. EM mcmorrow@ccs.nrl.navy.mil NR 13 TC 14 Z9 15 U1 1 U2 6 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855 USA SN 0018-9499 J9 IEEE T NUCL SCI JI IEEE Trans. Nucl. Sci. PD AUG PY 2006 VL 53 IS 4 BP 1819 EP 1824 DI 10.1109/TNS.2006.880929 PN 1 PG 6 WC Engineering, Electrical & Electronic; Nuclear Science & Technology SC Engineering; Nuclear Science & Technology GA 080JD UT WOS:000240242800012 ER PT J AU Xapsos, MA Stauffer, C Barth, JL Burke, EA AF Xapsos, M. A. Stauffer, C. Barth, J. L. Burke, E. A. TI Solar particle events and self-organized criticality: Are deterministic predictions of events possible? SO IEEE TRANSACTIONS ON NUCLEAR SCIENCE LA English DT Article; Proceedings Paper CT 8th European Conference on Radiation and Its Effects on Components and Systems CY SEP 19-23, 2005 CL Cap d Agde, FRANCE SP Univ Montpellier II DE fractal; rescaled range; self-organized criticality; solar particle event ID FLARES; MODEL; AVALANCHES AB Evidence is presented that solar particle events are a self-organized critical phenomenon. Using daily and monthly fluences of solar protons measured by the IMP-8 and GOES satellite instrumentation over a 28-year period, long-term correlation of events, fractal characteristics and power function behavior for the density functions of fluence magnitudes and waiting times are demonstrated. The implications are that it is not possible to predict the time of occurrence and magnitude of solar particle events within narrow limits. C1 NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Muniz Engn Inc, Seabrook, MD 20706 USA. RP Xapsos, MA (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. EM Michael.A.Xapsos@nasa.gov NR 17 TC 9 Z9 9 U1 0 U2 2 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855 USA SN 0018-9499 J9 IEEE T NUCL SCI JI IEEE Trans. Nucl. Sci. PD AUG PY 2006 VL 53 IS 4 BP 1839 EP 1843 DI 10.1109/TNS.2006.880576 PN 1 PG 5 WC Engineering, Electrical & Electronic; Nuclear Science & Technology SC Engineering; Nuclear Science & Technology GA 080JD UT WOS:000240242800015 ER PT J AU Warner, JH Messenger, SR Walters, RJ Summers, GP Lorentzen, JR Wilt, DM Smith, MA AF Warner, Jeffrey H. Messenger, Scott R. Walters, Robert J. Summers, Geoffrey P. Lorentzen, Justin R. Wilt, David M. Smith, Mark A. TI Correlation of electron radiation induced-damage in GaAs solar cells SO IEEE TRANSACTIONS ON NUCLEAR SCIENCE LA English DT Article; Proceedings Paper CT 8th European Conference on Radiation and its Effects on Components and Systems CY SEP 19-23, 2005 CL Cap d Agde, FRANCE SP Univ Montpellier II DE damage correlation; displacement damage; electron displacement damage; GaAs solar cells; nonionizing energy loss (NIEL); radiation damage ID LIGHT-EMITTING-DIODES; ENERGY-DEPENDENCE; DISPLACEMENT DAMAGE; PROTON IRRADIATION; LIFETIME; NIEL AB GaAs solar cells with different structures and polarities were irradiated with 1 and 5 MeV electrons. The energy dependence of the electron damage coefficients for the photocurrent, photovoltage, and maximum power were found to vary approximately linearly with NIEL in contrast to what has been found for other GaAs cells. C1 USN, Res Lab, Washington, DC 20375 USA. Univ Maryland Baltimore Cty, Baltimore, MD 21250 USA. SFA Inc, Largo, MD 20774 USA. Univ Maryland Baltimore Cty, Dept Phys, Baltimore, MD 21253 USA. NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. OAI, Cleveland, OH 44142 USA. RP Warner, JH (reprint author), USN, Res Lab, Washington, DC 20375 USA. EM jwarne4@umbc.edu; senger@nrl.navy.mil; rwalters@ccs.nrl.navy.mil; gsummers@ccf.nrl.navy.mil; jlorentz@estd.nrl.navy.mil; david.wilt@grc.nasa.gov; Mark.A.Smith@grc.nasa.gov NR 24 TC 21 Z9 22 U1 0 U2 5 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855 USA SN 0018-9499 J9 IEEE T NUCL SCI JI IEEE Trans. Nucl. Sci. PD AUG PY 2006 VL 53 IS 4 BP 1988 EP 1994 DI 10.1109/TNS.2006.877877 PN 1 PG 7 WC Engineering, Electrical & Electronic; Nuclear Science & Technology SC Engineering; Nuclear Science & Technology GA 080JD UT WOS:000240242800037 ER PT J AU Rezgui, S Swift, GM Lesea, A AF Rezgui, Sana Swift, Gary M. Lesea, Austin TI Characterization of upset-induced degradation of error-mitigated high-speed I/O's using fault injection on SRAM based FPGAs SO IEEE TRANSACTIONS ON NUCLEAR SCIENCE LA English DT Article; Proceedings Paper CT 8th European Conference on Radiation and its Effects on Components and Systems CY SEP 19-23, 2005 CL Cap d Agde, FRANCE SP Univ Montpellier II DE fault injection; field programmable gate arrays (FPGAs); upset mitigation; upset simulation AB Fault-injection experiments on Virtex-II (TM) FPGAs quantify failure and degradation modes in I/O channels incorporating triple module redundancy (TMR). With increasing frequency (to 100 MHz), full TMR under both 1/0 standards investigated (LVCMOS at 3.3V and 1.8V) shows more configuration bits have a measurable detrimental performance effect when in error. C1 Xilinx Inc, San Jose, CA 95124 USA. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Rezgui, S (reprint author), Xilinx Inc, San Jose, CA 95124 USA. EM sana.rezgui@xilinx.com; gary.m.swift@jpl.nasa.gov NR 6 TC 2 Z9 3 U1 0 U2 1 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855 USA SN 0018-9499 J9 IEEE T NUCL SCI JI IEEE Trans. Nucl. Sci. PD AUG PY 2006 VL 53 IS 4 BP 2076 EP 2083 DI 10.1109/TNS.2006.876510 PN 1 PG 8 WC Engineering, Electrical & Electronic; Nuclear Science & Technology SC Engineering; Nuclear Science & Technology GA 080JD UT WOS:000240242800050 ER PT J AU Eichler, T Rind, D Zebiak, S AF Eichler, Timothy Rind, David Zebiak, Stephen TI Impact of global warming on ENSO variability using the coupled GISS GCM/ZC model SO INTERNATIONAL JOURNAL OF CLIMATOLOGY LA English DT Article DE El Nino; STC; teleconnections; dynamical thermostat; upwelling; global warming; SST; equilibrium climate ID NINO-SOUTHERN-OSCILLATION; GENERAL-CIRCULATION MODEL; SEA-SURFACE TEMPERATURE; OCEAN-ATMOSPHERE MODEL; CLIMATE SYSTEM MODEL; EL-NINO; TROPICAL PACIFIC; INCREASED CO2; DECADAL VARIABILITY; GODDARD-INSTITUTE AB This study uses a hybrid coupled model (referred to as the general-circulation model (GCM)/Zebiak/Cane (ZC) model), which consists of the Goddard Institute for Space Studies' (GISS) Atmospheric general-circulation model (AGCM) coupled to the oceanic component of the ZC intermediate model to assess the impact of global warming on El Nino behavior, with and without the influence of heat introduced from the subtropical Pacific (via subtropical cell (STC) pathway). The baseline GCM/ZC model produces El Nino variability with a two year periodicity and an amplitude of approximately half the magnitude of observed El Nino. The GCM/ZC model also produces an appropriate atmospheric global response to El Nino/southern oscillation (ENSO) as shown by composites of 500 hPa heights, sea-level pressure (SLP), 200 hPa wind, and precipitation during El Nino and La Nina periods. To evaluate the importance of global warming on ENSO variability, 2x CO2 and 4x CO2 transient simulations were done increasing the atmospheric CO2 one percent per year, then extending the runs for an additional 70 years to obtain equilibrium climates for each run. An additional set of global-warming simulations was run after including a STC parameterization generated by computing 5-year running means of the sea-surface temperature (SST) difference between a transient run and the 1 x CO2 GCM/ZC run at the anticipated subduction zones (160-130 degrees W, 20-40 degrees N and 20-44 degrees S, 160-130 degrees W) and adding it to the base of the equatorial mixed-layer of the ZC model with a time lag of 15 years. This effectively alters the vertical temperature gradient of the ZC model, which affects SST via upwelling. Two features of the GCM/ZC response to global warming are emphasized. Firstly, the inclusion of the STC results in a major redistribution of heat across the equatorial Pacific, leading to an El Nino-like response in the final equilibrium solution with less variability about the mean. The global warming aspect due to the El Nino-like response results in a positive feedback on global warming, which causes a higher global surface-air temperature (SAT) than identical transient simulations without inclusion of the STC. Secondly, including the STC effect produces a far greater magnitude of global ENSO-like impact because of the reduction of, or even the reversal of, the equatorial Pacific longitudinal SST gradient. The implications of such an extreme climate scenario are discussed. Copyright (C) 2006 Royal Meteorological Society. C1 NASA, Goddard Inst Space Studies, New York, NY 10025 USA. Lamont Doherty Earth Observ, Palisades, NY 10964 USA. RP Eichler, T (reprint author), NOAA, OAR, 1315 East West Highway, Silver Spring, MD 20910 USA. EM tim.eichler@noaa.gov RI Eichler, Timothy/A-5040-2015 OI Eichler, Timothy/0000-0003-0342-9681 NR 56 TC 2 Z9 2 U1 3 U2 10 PU JOHN WILEY & SONS LTD PI CHICHESTER PA THE ATRIUM, SOUTHERN GATE, CHICHESTER PO19 8SQ, W SUSSEX, ENGLAND SN 0899-8418 J9 INT J CLIMATOL JI Int. J. Climatol. PD AUG PY 2006 VL 26 IS 10 BP 1283 EP 1314 DI 10.1002/joc.1308 PG 32 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 072JP UT WOS:000239670000001 ER PT J AU Kreuzinger, J Friedrich, R Gatski, TB AF Kreuzinger, Johannes Friedrich, Rainer Gatski, Thomas B. TI Compressibility effects in the solenoidal dissipation rate equation: A priori assessment and modeling SO INTERNATIONAL JOURNAL OF HEAT AND FLUID FLOW LA English DT Article; Proceedings Paper CT 4th International Symposium on Turbulence and Shear Flow Phenomena CY JUN 27-29, 2005 CL Williamsburg, VA DE solenoidal dissipation rate equation; direct numerical simulation; compressibility effects; modeling the baroclinic term ID TURBULENT SHEAR-FLOW; DIRECT-NUMERICAL-SIMULATION; LOW-REYNOLDS-NUMBER; CHANNEL FLOW; STRESS AB Several attempts have been made in the literature to improve the ability of statistical models to predict turbulent compressible flows. As yet, it is not possible to accurately predict both free and wall-bounded flows with the same model under a variety of conditions. One drawback in these attempts has been the lack of sufficiently reliable data with which to assess the various terms arising in the compressible turbulent transport equations. In this study, the exact terms of the solenoidal dissipation rate equation are calculated for the first time in both a compressible channel flow and a turbulent mixing layer. This data is then used to assess both the exact and modeled form of this equation. In its exact form, terms explicitly dependent on dilatation fluctuations and density and viscosity gradients appear. In addition, the terms that are also present in the incompressible equation now may vary differently under increased compressibility conditions. This latter effect can be either an indirect one, that is compressibility modifies mean quantities and Reynolds stresses, or a direct one, that is the processes in the solenoidal dissipation rate equation are themselves modified by compressibility. In order to separate the indirect and direct effects, it is assumed that the processes in the solenoidal dissipation rate equation are properly described by the available incompressible functional forms. The model coefficients are then determined by a priori tests. Direct effects appear if the coefficients depend on compressibility. These effects have then to be modeled additionally. (C) 2006 Elsevier Inc. All rights reserved. C1 Tech Univ Munich, Fachgebiet Stromungsmech, D-85747 Garching, Germany. NASA, Computat Aerosci Branch, Langley Res Ctr, Hampton, VA 23681 USA. RP Friedrich, R (reprint author), Tech Univ Munich, Fachgebiet Stromungsmech, D-85747 Garching, Germany. EM r.friedrich@lrz.tum.de; t.b.gatski@larc.nasa.gov NR 19 TC 9 Z9 9 U1 0 U2 1 PU ELSEVIER SCIENCE INC PI NEW YORK PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA SN 0142-727X J9 INT J HEAT FLUID FL JI Int. J. Heat Fluid Flow PD AUG PY 2006 VL 27 IS 4 BP 696 EP 706 DI 10.1016/j.ijheatfluidflow.2006.02.014 PG 11 WC Thermodynamics; Engineering, Mechanical; Mechanics SC Thermodynamics; Engineering; Mechanics GA 074SM UT WOS:000239832100020 ER PT J AU Copland, E AF Copland, Evan TI Comparing the thermodynamic behaviour of Al(l)+ZrO2(4% Y2O3) and Al(l)+Al2O3 SO INTERNATIONAL JOURNAL OF MATERIALS RESEARCH LA English DT Article DE KEMS; thermodynamic property measurements; Al(g); Al2O(g); Al-Zr-O system ID SYSTEM; PRESSURES; AL-AL2O3 AB In an effort to better determine the thermodynamic properties of Al(g) and Al2O(g) the vapour in equilibrium with Al(1) + 4 at.% yttria-stabilized zirconia (YSZ) was compared to the vapour in equilibrium with Al(l) + Al2O3(S) over the temperature range 1197 - 1509 K. This comparison was made directly by Knudsen effusion-cell mass spectrometry with an instrument configured for a multiple effusion-cell vapour source (multi-cell KEMS). Second-law enthalpies of vaporization of Al(g) and Al2O(g) together with activity measurements show that Al(l) + YSZ is thermodynamically equivalent to Al(l) + Al2O3(s), indicating that Al(l) remained pure and Al2O3(S) was present in the YSZ-cell. Subsequent observation of the Al(l)/YSZ and vapour/YSZ interfaces revealed a thin Al2O3-layer had formed, separating the YSZ-cell from Al(l) and Al(g) + Al2O(g), effectively transforming it into an Al2O3 effusion-cell. This behaviour agreed with observations made for beta-NiAl(Pt) alloys measured in YSZ effusion-cell. C1 Case Western Reserve Univ, NASA, Glenn Res Ctr, Dept Mat Sci & Engn, Cleveland, OH 44135 USA. RP Copland, E (reprint author), Case Western Reserve Univ, NASA, Glenn Res Ctr, Dept Mat Sci & Engn, 21000 Brookpk Rd,Mail Stop 106-1, Cleveland, OH 44135 USA. EM Evan.Copland@grc.nasa.gov NR 23 TC 1 Z9 1 U1 0 U2 1 PU CARL HANSER VERLAG PI MUNICH PA KOLBERGERSTRASSE 22, POSTFACH 86 04 20, D-81679 MUNICH, GERMANY SN 1862-5282 J9 INT J MATER RES JI Int. J. Mater. Res. PD AUG PY 2006 VL 97 IS 8 BP 1108 EP 1114 PG 7 WC Metallurgy & Metallurgical Engineering SC Metallurgy & Metallurgical Engineering GA 084OT UT WOS:000240543500007 ER PT J AU Hasanyan, DJ Librescu, L Ambur, DR AF Hasanyan, Davresh J. Librescu, Liviu Ambur, Damodar R. TI Buckling and postbuckling of magnetoelastic flat plates carrying an electric current SO INTERNATIONAL JOURNAL OF SOLIDS AND STRUCTURES LA English DT Article DE magnetoelastic plates; electrical current; buckling and postbuckling; snap-through; frequency-electrical current interaction ID FERROMAGNETIC ELASTIC SOLIDS; MAGNETIC-FIELD; CURVED PANELS; VIBRATION AB The basic equations of a fully nonlinear theory of electromagnetically conducting flat plates carrying an electric current and exposed to a magnetic field of arbitrary orientation are derived. The relevant equations have been obtained by considering that both the elastic and electromagnetic media are homogeneous and isotropic. The geometrical nonlinearities are considered in the von-Karman sense, and the soft ferromagnetic material of the plate is assumed to feature negligible hysteretic losses. Based on the electromagnetic and elastokinetic field equations, by using the standard averaging methods, the 3-D coupled problem is reduced to an equivalent 2-D one, appropriate to the theory of plates. Having in view that the elastic structures carrying an electric current are prone to buckling, by using the presently developed theory, the associated problems of buckling and postbuckling are investigated. In this context, the problem of the electrical current inducing the buckling instability of the plate, and its influence on the postbuckling behavior are analyzed. In the same context, the problem of the natural frequency-electrical current interaction of flat plates, as influenced by a magnetic field is also addressed. (c) 2005 Published by Elsevier Ltd. C1 Virginia Polytech Inst & State Univ, Blacksburg, VA 24061 USA. NASA, Langley Res Ctr, Hampton, VA 23681 USA. RP Librescu, L (reprint author), Virginia Polytech Inst & State Univ, Blacksburg, VA 24061 USA. EM dhasanya@vt.edu; librescu@vt.edu NR 33 TC 12 Z9 21 U1 1 U2 1 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0020-7683 J9 INT J SOLIDS STRUCT JI Int. J. Solids Struct. PD AUG PY 2006 VL 43 IS 16 BP 4971 EP 4996 DI 10.1016/j.ijsolstr.2005.04.028 PG 26 WC Mechanics SC Mechanics GA 061MO UT WOS:000238876800019 ER PT J AU Satomi, M La Duc, MT Venkateswaran, K AF Satomi, Masataka La Duc, Myron T. Venkateswaran, Kasthuri TI Bacillus safensis sp nov., isolated from spacecraft and assembly-facility surfaces SO INTERNATIONAL JOURNAL OF SYSTEMATIC AND EVOLUTIONARY MICROBIOLOGY LA English DT Article ID MARS ODYSSEY SPACECRAFT; 16S RIBOSOMAL-RNA; POLYPHASIC TAXONOMY; GYRB GENES; AMPLIFICATION; SHEWANELLA; SEQUENCES; ALIGNMENT; BACTERIA; STRAINS AB Thirteen strains of a novel spore-forming, Gram-positive, mesophilic heterotrophic bacterium were isolated from spacecraft surfaces (Mars Odyssey Orbiter) and assembly-facility surfaces at the Jet Propulsion Laboratory in California and the Kennedy Space Center in Florida. Phylogenetic analysis of 16S rRNA gene sequences has placed these novel isolates within the genus Bacillus, the greatest sequence similarity (99-90%) being found with Bacillus pumilus. However, these isolates share a mere 91(.)2 % gyrB sequence similarity with Bacillus pumilus, rendering their 16S rRNA gene-derived relatedness suspect. Furthermore, DNA-DNA hybridization showed only 54-66 % DNA relatedness between the novel isolates and strains of B. pumilus. rep-PCR fingerprinting and previously reported matrix-assisted laser desorption/ionization time-of-flight mass spectrometry protein profiling clearly distinguished these isolates from B. pumilus. Phenotypic analyses also showed some differentiation between the two genotypic groups, although the fatty acid compositions were almost identical. The polyphasic taxonomic studies revealed distinct clustering of the tested strains into two distinct species. On the basis of phenotypic characteristics and the results of phylogenetic analyses of 16S rRNA and gyrB gene sequences, repetitive element primer-PCR fingerprinting and DNA-DNA hybridization, the 13 isolates represent a novel species of the genus Bacillus, for which the name Bacillus safensis sp. nov. is proposed. The type strain is FO-36b(T) (= ATCC BAA-1126(T) = NBRC 100820(T)). C1 CALTECH, Jet Prop Lab, Biotechnol & Planetary Protect Grp, Pasadena, CA 91109 USA. Fisheries Res Agcy, Natl Res Inst Fisheries Sci, Yokohama, Kanagawa 2368648, Japan. RP Venkateswaran, K (reprint author), CALTECH, Jet Prop Lab, Biotechnol & Planetary Protect Grp, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM kjvenkat@jpl.nasa.gov NR 33 TC 58 Z9 62 U1 2 U2 10 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 AUG PY 2006 VL 56 BP 1735 EP 1740 DI 10.1099/ijs.0.64189-0 PN 8 PG 6 WC Microbiology SC Microbiology GA 079OA UT WOS:000240185200003 PM 16902000 ER PT J AU Chiu, JC Petty, GW AF Chiu, J. Christine Petty, Grant W. TI Bayesian retrieval of complete posterior PDFs of oceanic rain rate from microwave observations SO JOURNAL OF APPLIED METEOROLOGY AND CLIMATOLOGY LA English DT Article ID PRECIPITATION PROFILE RETRIEVAL; MEASURING MISSION; PHYSICAL RETRIEVALS; ALGORITHM; DISTRIBUTIONS; CLOUD; RADIOMETRY; PARAMETERS; IMAGERY; RADAR AB A new Bayesian algorithm for retrieving surface rain rate from Tropical Rainfall Measuring Mission (TRMM) Microwave Imager (TMI) over the ocean is presented, along with validations against estimates from the TRMM Precipitation Radar (PR). The Bayesian approach offers a rigorous basis for optimally combining multichannel observations with prior knowledge. While other rain-rate algorithms have been published that are based at least partly on Bayesian reasoning, this is believed to be the first self-contained algorithm that fully exploits Bayes's theorem to yield not just a single rain rate, but rather a continuous posterior probability distribution of rain rate. To advance the understanding of theoretical benefits of the Bayesian approach, sensitivity analyses have been conducted based on two synthetic datasets for which the "true" conditional and prior distribution are known. Results demonstrate that even when the prior and conditional likelihoods are specified perfectly, biased retrievals may occur at high rain rates. This bias is not the result of a defect of the Bayesian formalism, but rather represents the expected outcome when the physical constraint imposed by the radiometric observations is weak owing to saturation effects. It is also suggested that both the choice of the estimators and the prior information are crucial to the retrieval. In addition, the performance of the Bayesian algorithm herein is found to be comparable to that of other benchmark algorithms in real-world applications, while having the additional advantage of providing a complete continuous posterior probability distribution of surface rain rate. C1 Univ Maryland Baltimore Cty, Joint Ctr Earth Syst Technol, Baltimore, MD 21228 USA. Univ Wisconsin, Dept Atmospher & Ocean Sci, Madison, WI USA. RP Chiu, JC (reprint author), NASA, Goddard Space Flight Ctr, Code 613-2, Greenbelt, MD 20771 USA. EM cchiu@climate.gsfc.nasa.gov RI Petty, Grant/E-3118-2012; Chiu, Christine/E-5649-2013 OI Chiu, Christine/0000-0002-8951-6913 NR 32 TC 13 Z9 13 U1 0 U2 2 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 AUG PY 2006 VL 45 IS 8 BP 1073 EP 1095 DI 10.1175/JAM2392.1 PG 23 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 085RN UT WOS:000240622200004 ER PT J AU Jiang, HY Zipser, EJ AF Jiang, Haiyan Zipser, Edward J. TI Retrieval of hydrometeor profiles in tropical cyclones and convection from combined radar and radiometer observations SO JOURNAL OF APPLIED METEOROLOGY AND CLIMATOLOGY LA English DT Article ID PASSIVE MICROWAVE OBSERVATIONS; REMOTE-SENSING APPLICATIONS; VERTICAL VELOCITY EVENTS; MEASURING MISSION TRMM; MELTING-LAYER MODEL; SIZE DISTRIBUTIONS; PART I; LIGHTNING CHARACTERISTICS; PRECIPITATION PROFILES; OCEANIC CONVECTION AB A retrieval algorithm is described to estimate vertical profiles of precipitation ice water content and liquid water content in tropical cyclones and convection over ocean from combined spaceborne radar and radiometer measurements. In the algorithm, the intercept parameter N(0)s in the exponential particle size distribution for rain, snow, and graupel are adjusted iteratively to minimize the difference between observed brightness temperatures and simulated ones by using a simulated annealing optimization method. Sensitivity tests are performed to understand the effects of the input parameters. The retrieval technique is investigated using the Earth Resources (ER)-2 aircraft Doppler radar and Advanced Microwave Precipitation Radiometer data in tropical cyclones and convection. An indirect validation is performed by comparing the measured and retrieved 50-GHz (independent channel) brightness temperature. The global agreement shows not only the quality of the inversion procedure, but also the consistency of the retrieved parameters with observations. The direct validation of the ice water content retrieval by using the aircraft in situ microphysical measurements indicates that the algorithm can provide reliable ice water content estimates, especially in stratiform regions. In convective regions, the large variability of the microphysical characteristics causes a large uncertainty in the retrieval, although the mean difference between the retrieved ice water content and aircraft-derived ice water content is very small. The ice water content estimated by a radar-only empirical relationship is higher than those retrieved by the combined algorithm and derived by the aircraft in situ observations. The new combined algorithm contains information that should improve ice water content estimates from either radar-only or passive microwave-only measurements. An important caveat for this study is that it concerns precipitation estimates. In this paper, ice and liquid water content should be interpreted as precipitation ice and liquid water content. C1 Univ Utah, Dept Meteorol, Salt Lake City, UT 84112 USA. RP Jiang, HY (reprint author), NASA, Goddard Space Flight Ctr, Code 613-1,Bldg 33,Rm C415, Greenbelt, MD 20771 USA. EM jiang@agnes.gsfc.nasa.gov NR 74 TC 10 Z9 10 U1 1 U2 7 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 AUG PY 2006 VL 45 IS 8 BP 1096 EP 1115 DI 10.1175/JAM2386.1 PG 20 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 085RN UT WOS:000240622200005 ER PT J AU Ruzmaikin, A Cadavid, AC Lawrence, JK AF Ruzmaikin, Alexander Cadavid, Ana Cristina Lawrence, John K. TI Stratospheric wave-mean flow interaction: Simple modeling SO JOURNAL OF ATMOSPHERIC AND SOLAR-TERRESTRIAL PHYSICS LA English DT Article DE atmosphere; middle atmosphere dynamics; stratosphere/troposphere interactions; planetary waves ID NORTHERN-HEMISPHERE WINTER; SOLAR VARIABILITY; ATMOSPHERE; REGIMES; CLIMATE; MODES; SUN AB We show that the interaction between planetary waves and the stratospheric zonal mean flow results in bi-modal (directreverse flow) or unimodal state depending on wave number of the waves. First we demonstrate this using a simple nonlinear dynamic system of the wave-flow interaction, which has two stable equilibrium states and one unstable state (attractors) in its phase space. Then we compare this model dynamics with the stratosphere dynamics using the same dynamical variables and a similar parameter range in the National Centers for Environmental Prediction (NCEP) Reanalysis data. This comparison supports the tendency for the states of planetary wave-zonal mean flow in the upper stratosphere to be bi-modal for wave number 2 and unimodal for wave number 1. Crown Copyright (c) 2006 Published by Elsevier Ltd. All rights reserved. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. Calif State Univ Northridge, Dept Phys & Astron, Northridge, CA 91330 USA. RP Ruzmaikin, A (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91125 USA. EM Alexander.Ruzmaikin@jpl.nasa.gov NR 25 TC 4 Z9 4 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 AUG PY 2006 VL 68 IS 12 BP 1311 EP 1320 DI 10.1016/j.jastp.2006.05.004 PG 10 WC Geochemistry & Geophysics; Meteorology & Atmospheric Sciences SC Geochemistry & Geophysics; Meteorology & Atmospheric Sciences GA 079GV UT WOS:000240164800003 ER PT J AU Bony, S Colman, R Kattsov, VM Allan, RP Bretherton, CS Dufresne, JL Hall, A Hallegatte, S Holland, MM Ingram, W Randall, DA Soden, BJ Tselioudis, G Webb, MJ AF Bony, Sandrine Colman, Robert Kattsov, Vladimir M. Allan, Richard P. Bretherton, Christopher S. Dufresne, Jean-Louis Hall, Alex Hallegatte, Stephane Holland, Marika M. Ingram, William Randall, David A. Soden, Brian J. Tselioudis, George Webb, Mark J. TI How well do we understand and evaluate climate change feedback processes? SO JOURNAL OF CLIMATE LA English DT Review ID GENERAL-CIRCULATION MODELS; WATER-VAPOR FEEDBACK; SEA-SURFACE TEMPERATURE; UPPER-TROPOSPHERIC HUMIDITY; RADIATION BUDGET EXPERIMENT; CLOUD LIQUID WATER; ICE-THICKNESS DISTRIBUTION; LARGE-SCALE CIRCULATION; SNOW-ALBEDO FEEDBACK; RELATIVE-HUMIDITY AB Processes in the climate system that can either amplify or dampen the climate response to an external perturbation are referred to as climate feedbacks. Climate sensitivity estimates depend critically on radiative feedbacks associated with water vapor, lapse rate, clouds, snow, and sea ice, and global estimates of these feedbacks differ among general circulation models. By reviewing recent observational, numerical, and theoretical studies, this paper shows that there has been progress since the Third Assessment Report of the Intergovernmental Panel on Climate Change in (i) the understanding of the physical mechanisms involved in these feedbacks, (ii) the interpretation of intermodel differences in global estimates of these feedbacks, and (iii) the development of methodologies of evaluation of these feedbacks ( or of some components) using observations. This suggests that continuing developments in climate feedback research will progressively help make it possible to constrain the GCMs' range of climate feedbacks and climate sensitivity through an ensemble of diagnostics based on physical understanding and observations. C1 CNRS, IPSL, LMD, F-75252 Paris 05, France. Bur Meteorol Res Ctr, Melbourne, Vic, Australia. Voeikov Main Geophys Observ, St Petersburg, Russia. Univ Reading, Environm Syst Sci Ctr, Reading, Berks, England. Univ Washington, Dept Atmospher Sci, Seattle, WA 98195 USA. Univ Calif Los Angeles, Dept Atmospher & Ocean Sci, Los Angeles, CA USA. Ctr Int Rech Environm & Dev, Nogent Sur Marne, France. Meteo France, Ctr Natl Rech Meteorol, Toulouse, France. Natl Ctr Atmospher Res, Boulder, CO 80307 USA. Univ Oxford, Clarendon Lab, Oxford OX1 3PU, England. Met Off, Hadley Ctr Climate Predict & Res, Exeter, Devon, England. Colorado State Univ, Dept Atmospher Sci, Ft Collins, CO 80523 USA. Univ Miami, Rosenstiel Sch Marine & Atmospher Sci, Miami, FL 33149 USA. Columbia Univ, NASA GISS, New York, NY USA. Columbia Univ, Dept Appl Phys, New York, NY USA. RP Bony, S (reprint author), CNRS, IPSL, LMD, Boite 99,4 Pl Jussieu, F-75252 Paris 05, France. EM bony@lmd.jussieu.fr RI Hall, Alex/D-8175-2014; Dufresne, Jean-Louis/I-5616-2015; Allan, Richard/B-5782-2008; Randall, David/E-6113-2011 OI Dufresne, Jean-Louis/0000-0003-4764-9600; Bony, Sandrine/0000-0002-4791-4438; Allan, Richard/0000-0003-0264-9447; Randall, David/0000-0001-6935-4112 NR 231 TC 448 Z9 462 U1 11 U2 125 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 0894-8755 EI 1520-0442 J9 J CLIMATE JI J. Clim. PD AUG PY 2006 VL 19 IS 15 BP 3445 EP 3482 DI 10.1175/JCLI3819.1 PG 38 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 076FT UT WOS:000239943100001 ER PT J AU Wong, T Wielicki, BA Lee, RB, Smith, GL Bush, KA Willis, JK AF Wong, Takmeng Wielicki, Bruce A. Lee, Robert B., III Smith, G. Louis Bush, Kathryn A. Willis, Joshua K. TI Reexamination of the observed decadal variability of the earth radiation budget using altitude-corrected ERBE/ERBS nonscanner WFOV data SO JOURNAL OF CLIMATE LA English DT Article ID ANTHROPOGENIC CLIMATE-CHANGE; OUTGOING LONGWAVE RADIATION; EXPERIMENT ERBE; DATA SET; INSTRUMENT; CLOUDS; MODEL; CALIBRATION; SYSTEM; IMPACT AB This paper gives an update on the observed decadal variability of the earth radiation budget (ERB) using the latest altitude-corrected Earth Radiation Budget Experiment (ERBE)/Earth Radiation Budget Satellite (ERBS) Nonscanner Wide Field of View (WFOV) instrument Edition3 dataset. The effects of the altitude correction are to modify the original reported decadal changes in tropical mean (20 degrees N to 20 degrees S) longwave (LW), shortwave (SW), and net radiation between the 1980s and the 1990s from 3.1, -2.4, and -0.7 to 1.6, -3.0, and 1.4 W m(-2), respectively. In addition, a small SW instrument drift over the 15-yr period was discovered during the validation of the WFOV Edition3 dataset. A correction was developed and applied to the Edition3 dataset at the data user level to produce the WFOV Edition3_Rev1 dataset. With this final correction, the ERBS Nonscanner-observed decadal changes in tropical mean LW, SW, and net radiation between the 1980s and the 1990s now stand at 0.7, -2.1, and 1.4 W m(-2), respectively, which are similar to the observed decadal changes in the High-Resolution Infrared Radiometer Sounder (HIRS) Pathfinder OLR and the International Satellite Cloud Climatology Project (ISCCP) version FD record but disagree with the Advanced Very High Resolution Radiometer (AVHRR) Pathfinder ERB record. Furthermore, the observed interannual variability of near-global ERBS WFOV Edition3_Rev1 net radiation is found to be remarkably consistent with the latest ocean heat storage record for the overlapping time period of 1993 to 1999. Both datasets show variations of roughly 1.5 W m(-2) in planetary net heat balance during the 1990s. C1 NASA, Langley Res Ctr, Hampton, VA 23681 USA. Natl Inst Aerosp, Hampton, VA USA. Sci Applicat Int Corp, Hampton, VA USA. CALTECH, Jet Prop Lab, Pasadena, CA USA. RP Wong, T (reprint author), NASA, Langley Res Ctr, MS 420, Hampton, VA 23681 USA. EM takmeng.wong@nasa.gov NR 36 TC 89 Z9 89 U1 0 U2 4 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 0894-8755 EI 1520-0442 J9 J CLIMATE JI J. Clim. PD AUG PY 2006 VL 19 IS 16 BP 4028 EP 4040 DI 10.1175/JCLI3838.1 PG 13 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 080DT UT WOS:000240228000015 ER PT J AU Sun, DZ Zhang, T Covey, C Klein, SA Collins, WD Hack, JJ Kiehl, JT Meehl, GA Held, IM Suarez, M AF Sun, D. -Z. Zhang, T. Covey, C. Klein, S. A. Collins, W. D. Hack, J. J. Kiehl, J. T. Meehl, G. A. Held, I. M. Suarez, M. TI Radiative and dynamical feedbacks over the equatorial cold tongue: Results from nine atmospheric GCMs SO JOURNAL OF CLIMATE LA English DT Article ID CLIMATE SYSTEM MODEL; GENERAL-CIRCULATION MODELS; 1986-87 EL-NINO; WATER-VAPOR; CUMULUS CONVECTION; CLOUD FEEDBACK; PART I; OCEAN; TEMPERATURE; GREENHOUSE AB The equatorial Pacific is a region with strong negative feedbacks. Yet coupled general circulation models (GCMs) have exhibited a propensity to develop a significant SST bias in that region, suggesting an unrealistic sensitivity in the coupled models to small energy flux errors that inevitably occur in the individual model components. Could this "hypersensitivity" exhibited in a coupled model be due to an underestimate of the strength of the negative feedbacks in this region? With this suspicion, the feedbacks in the equatorial Pacific in nine atmospheric GCMs (AGCMs) have been quantified using the interannual variations in that region and compared with the corresponding calculations from the observations. The nine AGCMs are the NCAR Community Climate Model version 1 (CAM1), the NCAR Community Climate Model version 2 (CAM2), the NCAR Community Climate Model version 3 (CAM3), the NCAR CAM3 at T85 resolution, the NASA Seasonal-to-Interannual Prediction Project (NSIPP) Atmospheric Model, the Hadley Centre Atmospheric Model (HadAM3), the Institut Pierre Simon Laplace (IPSL) model (LMDZ4), the Geophysical Fluid Dynamics Laboratory (GFDL) AM2p10, and the GFDL AM2p12. All the corresponding coupled runs of these nine AGCMs have an excessive cold tongue in the equatorial Pacific. The net atmospheric feedback over the equatorial Pacific in the two GFDL models is found to be comparable to the observed value. All other models are found to have a weaker negative net feedback from the atmosphere - a weaker regulating effect on the underlying SST than the real atmosphere. Except for the French (IPSL) model, a weaker negative feedback from the cloud albedo and a weaker negative feedback from the atmospheric transport are the two leading contributors to the weaker regulating effect from the atmosphere. The underestimate of the strength of the negative feedbacks by the models is apparently linked to an underestimate of the equatorial precipitation response. All models have a stronger water vapor feedback than that indicated in Earth Radiation Budget Experiment (ERBE) observations. These results confirm the suspicion that an underestimate of the regulatory effect from the atmosphere over the equatorial Pacific region is a prevalent problem. The results also suggest, however, that a weaker regulatory effect from the atmosphere is unlikely solely responsible for the hypersensitivity in all models. The need to validate the feedbacks from the ocean transport is therefore highlighted. C1 NOAA, Earth Syst Res Lab, Boulder, CO 80305 USA. CIRES, Climate Diagnost Ctr, Boulder, CO USA. Lawrence Livermore Natl Lab, Livermore, CA USA. Natl Ctr Atmospher Res, Boulder, CO 80307 USA. NOAA, Geophys Fluid Dynam Lab, Princeton, NJ USA. NASA, Greenbelt, MD USA. RP Sun, DZ (reprint author), NOAA, Earth Syst Res Lab, 325 Broadway, Boulder, CO 80305 USA. EM dezheng.sun@noaa.gov RI Collins, William/J-3147-2014; Klein, Stephen/H-4337-2016 OI Collins, William/0000-0002-4463-9848; Klein, Stephen/0000-0002-5476-858X NR 54 TC 42 Z9 44 U1 0 U2 8 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 AUG PY 2006 VL 19 IS 16 BP 4059 EP 4074 DI 10.1175/JCLI3835.1 PG 16 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 080DT UT WOS:000240228000017 ER PT J AU Chen, YH Aires, F Francis, JA Miller, JR AF Chen, Yonghua Aires, Filipe Francis, Jennifer A. Miller, James R. TI Observed relationships between arctic longwave cloud forcing and cloud parameters using a neural network SO JOURNAL OF CLIMATE LA English DT Article ID ANNUAL CYCLE; WATER-VAPOR; SURFACE; RETRIEVAL; SATELLITE; TRENDS; TEMPERATURE; MODELS; LIQUID; SYSTEM AB A neural network technique is used to quantify relationships involved in cloud-radiation feedbacks based on observations from the Surface Heat Budget of the Arctic (SHEBA) project. Sensitivities of longwave cloud forcing (CFL) to cloud parameters indicate that a bimodal distribution pattern dominates the histogram of each sensitivity. Although the mean states of the relationships agree well with those derived in a previous study, they do not often exist in reality. The sensitivity of CFL to cloud cover increases as the cloudiness increases with a range of 0.1-0.9 W m(-2)%(-1). There is a saturation effect of liquid water path (LWP) on CFL. The highest sensitivity of CFL to LWP corresponds to clouds with low LWP, and sensitivity decreases as LWP increases. The sensitivity of CFL to cloud-base height (CBH) depends on whether the clouds are below or above an inversion layer. The relationship is negative for clouds higher than 0.8 km at the SHEBA site. The strongest positive relationship corresponds to clouds with low CBH. The dominant mode of the sensitivity of CFL to cloud-base temperature (CBT) is near zero and corresponds to warm clouds with base temperatures higher than -9 degrees C. The low and high sensitivity regimes correspond to the summer and winter seasons, respectively, especially for LWP and CBT. Overall, the neural network technique is able to separate two distinct regimes of clouds that correspond to different sensitivities; that is, it captures the nonlinear behavior in the relationships. This study demonstrates a new method for evaluating nonlinear relationships between climate variables. It could also be used as an effective tool for evaluating feedback processes in climate models. C1 Rutgers State Univ, Inst Marine & Coastal Sci, New Brunswick, NJ 08903 USA. Univ Paris 06, CNRS, Inst Pierre Simon Laplace, Meteorol Dynam Lab, Paris, France. RP Chen, YH (reprint author), NASA, Goddard Inst Space Studies, 2880 Broadway, New York, NY 10025 USA. EM ychen@giss.nasa.gov NR 25 TC 14 Z9 14 U1 0 U2 2 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 AUG PY 2006 VL 19 IS 16 BP 4087 EP 4104 DI 10.1175/JCLI3839.1 PG 18 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 080DT UT WOS:000240228000019 ER PT J AU Chiou, EW Thomason, LW Chu, WP AF Chiou, E. W. Thomason, L. W. Chu, W. P. TI Variability of stratospheric water vapor inferred from SAGE II, HALOE, and Boulder (Colorado) balloon measurements SO JOURNAL OF CLIMATE LA English DT Article ID TROPICAL TROPOPAUSE TEMPERATURES; AEROSOL AB The variability of stratospheric water vapor between 1996 and 2004 has been studied using multiyear measurements from the Stratospheric Aerosol and Gas Experiment II ( SAGE II) version 6.2 dataset, the Halogen Occultation Experiment (HALOE) version 19 dataset, and the balloon-borne frost point hygrometer data record at Boulder, Colorado (40 degrees N, 105 W). The features derived from SAGE II and HALOE for 20 degrees latitudinal zones from 60 degrees S to 60 degrees N at various altitudes (16-34 km) show good quantitative agreement regarding the phases and magnitudes of annual, semiannual, and quasi-biennial oscillations (QBO). For the latitudinal zones 20 degrees-40 degrees and 40 degrees-60 degrees, the hemispheric asymmetry at 22 km with mainly QBO in the north and predominantly annual oscillations in the south has been revealed by both SAGE II and HALOE observations. Strong correlation exists between SAGE II and HALOE lower-stratospheric H(2)O anomalies over low latitudes and 100-hPa tropical zonal mean temperature anomalies. The correlation coefficients based on the 0-20 degrees S water vapor time series with H(2)O lagged by 2 months are 0.81 and 0.70 for HALOE and SAGE II, respectively. For 35 degrees-45 degrees N, SAGE II and HALOE show consistent trends generally varying from -0.05 to -0.02 ppmv yr(-1) between 16 and 34 km. The corresponding analyses based on frost point measurements over Boulder show insignificant trends. These trends are not strongly dependent on the end points of the analysis and stand in contrast to the positive trends reported in previous studies that include data records prior to 1994. For the lower stratosphere, investigations of the entire balloon-borne dataset over Boulder indicate higher values of mixing ratios after 1992-93 compared to the period 1980-92. In contrast, SAGE II monthly zonal mean measurements for 35 degrees-45 degrees N show insignificant differences between the periods 1987-89 and 1996-2004. C1 Sci Applicat Int Corp, Hampton, VA USA. NASA, Langley Res Ctr, Hampton, VA 23665 USA. RP Chiou, EW (reprint author), Adnet Syst Inc, 7515 Mission Dr,Suite A1C1, Lanham, MD 20706 USA. EM echiou@sesda2.com OI Thomason, Larry/0000-0002-1902-0840 NR 17 TC 2 Z9 2 U1 0 U2 0 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 AUG PY 2006 VL 19 IS 16 BP 4121 EP 4133 DI 10.1175/JCLI3841.1 PG 13 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 080DT UT WOS:000240228000021 ER PT J AU Fedele, F Hitt, DL AF Fedele, Francesco Hitt, Darren L. TI Transport, growth, and stability of disturbances in weakly rarefied channel flows SO JOURNAL OF COMPUTATIONAL AND THEORETICAL NANOSCIENCE LA English DT Article DE slip flow; stability; pulsatile pipe flow; Orr-Sommerfeld operator; Galerkin projection; non-normality; vortex tubes; energy growth ID PIPE POISEUILLE FLOW; MICROCHANNEL FLOWS; PRESSURE-GRADIENT; BOUNDARY-LAYERS; REYNOLDS-NUMBER; CIRCULAR PIPE; VISCOUS DRAG; TRANSITION; VELOCITY; SLIP AB Rarefied flow on the micro- and nano-scale can be strongly influenced by the surface roughness of the solid boundaries as measured by the tangential momentum accommodation coefficient sigma. These same surface effects can give rise to flow perturbations whose evolution, growth, and stability must be characterized. From a nanotechnology application standpoint, the design of micro/nanofluidic devices may require knowledge of the flow response to disturbances to ensure proper device operation. In the present study we examine the response of pulsatile pipe flows to axisymmetric disturbances under conditions of weakly rarefied flows ('slip regime') typically defined by Knudsen numbers Kn <= 0.3. An Orr-Sommerfeld equation is derived and solved by means of a Galerkin projection onto the approximate functional space spanned by a finite set of eigenfunctions derived in the longwave limit of the Orr-Sommerfeld operator. Results from Floquet stability analyses show that pulsatile slip flow is slightly more stable than the steady slip-flow for longwave disturbance with the stability characteristics being only weakly dependent on the Knudsen number. The flow structures corresponding to the largest energy growth are toroidal vortex tubes that are transported diffusively and convectively by the mean flow. The transient energy growth is found to slightly increase with the Knudsen number, indicating that the Orr-Sommerfeld operator for slip flow is more non-normal when compared to continuum-based no-slip flows. C1 Univ Vermont, Dept Mech Engn, Burlington, VT 05405 USA. Univ Maryland Baltimore Cty, Goddard Earth Sci & Technol Ctr, Baltimore, MD 21228 USA. NASA, Goddard Space Flight Ctr, Global Modelling & Assimilat Off, Washington, DC 20546 USA. RP Hitt, DL (reprint author), Univ Vermont, Dept Mech Engn, Burlington, VT 05405 USA. RI Fedele, Francesco/J-7651-2012 OI Fedele, Francesco/0000-0001-6403-4224 NR 28 TC 1 Z9 1 U1 0 U2 0 PU AMER SCIENTIFIC PUBLISHERS PI VALENCIA PA 26650 THE OLD RD, STE 208, VALENCIA, CA 91381-0751 USA SN 1546-1955 EI 1546-1963 J9 J COMPUT THEOR NANOS JI J. Comput. Theor. Nanosci. PD AUG PY 2006 VL 3 IS 4 BP 497 EP 505 PG 9 WC Chemistry, Multidisciplinary; Nanoscience & Nanotechnology; Materials Science, Multidisciplinary; Physics, Applied; Physics, Condensed Matter SC Chemistry; Science & Technology - Other Topics; Materials Science; Physics GA 087PA UT WOS:000240753100005 ER PT J AU Lu, YJ Partridge, C Meyyappan, M Li, J AF Lu, Yijiang Partridge, Christina Meyyappan, M. Li, Jing TI A carbon nanotube sensor array for sensitive gas discrimination using principal component analysis SO JOURNAL OF ELECTROANALYTICAL CHEMISTRY LA English DT Article DE carbon nanotube; gas sensor array; gas discrimination; signal processing; pattern recognition AB A carbon nanotube based gas sensor array was developed for discriminating gases and vapors. The sensor array was composed of 32 sensing elements with nanomaterials, e.g. pristine single walled carbon nanotubes (SWNTs), and SWNTs with different metal dopants and polymer coatings. This sensor array was exposed to NO2, HCN, HCl, Cl-2, acetone and benzene in parts per million (ppm) concentration levels. The array data was normalized and autoscaled for eliminating concentration and background noise, and ignoring outliers. The post processed array data was then subjected to a principal component analysis, a pattern recognition technique, for gas and vapor discrimination. All tested gases and vapors can be discriminated by their chemical nature in the low gas/vapor concentration at ppm levels using this carbon nanotube based sensor array. (c) 2006 Elsevier B.V. All rights reserved. C1 NASA, Ames Res Ctr, Ctr Nanotechnol, Moffett Field, CA 94035 USA. RP Li, J (reprint author), NASA, Ames Res Ctr, Ctr Nanotechnol, Moffett Field, CA 94035 USA. EM jingli@mail.arc.nasa.gov NR 11 TC 63 Z9 69 U1 4 U2 27 PU ELSEVIER SCIENCE SA PI LAUSANNE PA PO BOX 564, 1001 LAUSANNE, SWITZERLAND SN 0022-0728 J9 J ELECTROANAL CHEM JI J. Electroanal. Chem. PD AUG 1 PY 2006 VL 593 IS 1-2 BP 105 EP 110 DI 10.1016/j.jelechem.2006.03.056 PG 6 WC Chemistry, Analytical; Electrochemistry SC Chemistry; Electrochemistry GA 067IT UT WOS:000239295900013 ER PT J AU Bhagwat, V Xiao, YG Bhat, I Dutta, P Refaat, TF Abedin, MN Kumar, V AF Bhagwat, Vinay Xiao, Yegao Bhat, Ishwara Dutta, Partha Refaat, Tamer F. Abedin, M. Nurul Kumar, Vikram TI Analysis of leakage currents in MOCVD grown GaInAsSb based photodetectors operating at 2 mu m SO JOURNAL OF ELECTRONIC MATERIALS LA English DT Article DE GaInAsSb; photodetector; surface leakage ID CURRENT-VOLTAGE CHARACTERISTICS; MOLECULAR-BEAM EPITAXY; PASSIVATION TREATMENTS; INGAASSB; DIODES; PHOTODIODES; WAVELENGTH; ARRAYS; RANGE AB This paper reports the fabrication and characterization of GaInAsSb photodetectors operating at 2 mu m. At room temperature, the performance of these photodiodes under reverse bias conditions is limited by the surface leakage. A model has been developed to separate the bulk (diffusion and generation-recombination (g-r)) and the surface leakage contributions toward the total leakage current. By fitting this model to the experimental data, values of material parameters such as minority carrier diffusion length and lifetime have been estimated. The highest R(0)A of 55 Omega-cm(2) has been obtained with a responsivity of 0.44 A/W at 2 mu m. C1 Rensselaer Polytech Inst, Dept Elect Comp & Syst Engn, Ctr Integrated Elect, Troy, NY 12180 USA. NASA, Langley Res Ctr, Sci & Technol Corp, Hampton, VA 23681 USA. NASA, Langley Res Ctr, Laser & Electroopt Branch, Hampton, VA 23681 USA. Natl Phys Lab, New Delhi 110012, India. RP Bhagwat, V (reprint author), Rensselaer Polytech Inst, Dept Elect Comp & Syst Engn, Ctr Integrated Elect, Troy, NY 12180 USA. RI Kumar, Vikram/E-6476-2011 OI Kumar, Vikram/0000-0001-9038-8456 NR 22 TC 9 Z9 9 U1 0 U2 4 PU MINERALS METALS MATERIALS SOC PI WARRENDALE PA 184 THORN HILL RD, WARRENDALE, PA 15086 USA SN 0361-5235 J9 J ELECTRON MATER JI J. Electron. Mater. PD AUG PY 2006 VL 35 IS 8 BP 1613 EP 1617 DI 10.1007/s11664-006-0206-x PG 5 WC Engineering, Electrical & Electronic; Materials Science, Multidisciplinary; Physics, Applied SC Engineering; Materials Science; Physics GA 078AE UT WOS:000240072400002 ER PT J AU Sigler, MF Hulbert, LB Lunsford, CR Thompson, NH Burek, K O'Corry-Crowe, G Hirons, AC AF Sigler, M. F. Hulbert, L. B. Lunsford, C. R. Thompson, N. H. Burek, K. O'Corry-Crowe, G. Hirons, A. C. TI Diet of Pacific sleeper shark, a potential Steller sea lion predator, in the north-east Pacific Ocean SO JOURNAL OF FISH BIOLOGY LA English DT Article DE diet; predation; sea lion; sleeper shark ID SOMNIOSUS-PACIFICUS; STOMACH CONTENTS; ALASKA; ISOTOPES; BEHAVIOR; DNA; ONCORHYNCHUS; ANIMALS; SALMON; GULF AB Pacific sleeper sharks Somniosus pacificus were captured near Steller sea lion Eumetopias jubatus rookeries during the period when Steller sea lion pups are most vulnerable to Pacific sleeper shark predation (first water entrance and weaning). Analysis of stomach contents revealed that teleosts were the dominant prey in August and cephalopods were the dominant prey in May (n = 198). Marine mammals were found in 15% of stomachs regardless of season, but no Steller sea lion tissues were detected. Molecular genetic analysis identified grey whale Eschrichtius robustus and harbour seal Phoca vitulina remains in some Pacific sleeper shark stomachs. Most mammals were cetacean and at least 70% of the cetaceans were probably scavenged. Although Pacific sleeper shark and Steller sea lion ranges overlapped, so predation could potentially occur, the diet study suggested that predation on Steller sea lions is unlikely, at least when pups first enter the water or during weaning. Harbour seals were infrequent prey and may have been consumed alive. Pacific sleeper sharks consume fast-swimming prey like Pacific salmon Oncorhynchus sp., most likely live animals rather than scavenged animals. Pacific sleeper sharks appeared to be opportunistic consumers of the available prey and carrion, feeding both on the bottom and in the water column, and their diet shifted to teleosts and cetacean carrion as the fish grew larger. (c) 2006 The Fisheries Society of the British Isles (No claim to original US government works) C1 NOAA, Alaska Fisheries Sci Ctr, Auke Bay Lab, Natl Marine Fisheries Serv, Juneau, AK 99801 USA. Bartlett Reg Hosp, Juneau, AK 99801 USA. Alaska Vet Pathol Serv, Eagle River, AK 99577 USA. SW Fisheries Sci Ctr, Natl Marine Fisheries Serv, La Jolla, CA 92037 USA. Univ Alaska Fairbanks, Inst Marine Sci, Fairbanks, AK 99775 USA. RP Sigler, MF (reprint author), NOAA, Alaska Fisheries Sci Ctr, Auke Bay Lab, Natl Marine Fisheries Serv, 11305 Glacier Highway, Juneau, AK 99801 USA. EM mike.sigler@noaa.gov NR 29 TC 26 Z9 28 U1 5 U2 26 PU BLACKWELL PUBLISHING PI OXFORD PA 9600 GARSINGTON RD, OXFORD OX4 2DQ, OXON, ENGLAND SN 0022-1112 J9 J FISH BIOL JI J. Fish Biol. PD AUG PY 2006 VL 69 IS 2 BP 392 EP 405 DI 10.1111/j.1095-8649.2006.01096.x PG 14 WC Fisheries; Marine & Freshwater Biology SC Fisheries; Marine & Freshwater Biology GA 076MF UT WOS:000239961700005 ER PT J AU Hulbert, LB Sigler, MF Lunsford, CR AF Hulbert, L. B. Sigler, M. F. Lunsford, C. R. TI Depth and movement behaviour of the Pacific sleeper shark in the north-east Pacific Ocean SO JOURNAL OF FISH BIOLOGY LA English DT Article DE Alaska; foraging behaviour; movements; Pacific sleeper shark; satellite tagging; Somniosus pacificus ID STELLER SEA LIONS; SOMNIOSUS-MICROCEPHALUS; GREENLAND SHARKS; VERTICAL MOVEMENTS; SWIMMING BEHAVIOR; SIPHONOSTOMATOIDA; LERNAEOPODIDAE; ONCORHYNCHUS; CALIFORNIA; ATTACHMENT AB Satellite-linked radio telemetry was used to study the geographic movements and vertical movement behaviour of the Pacific sleeper shark Somniosus pacificus. The fish were tagged near Steller sea lion Eumetopias jubatus rookeries in the Gulf of Alaska during periods when Steller sea lions pups were most vulnerable to predation; when Steller sea lion pups first enter the water (July to August) and when Steller sea lion pups are weaned (April to May). Final locations recovered from most Pacific sleeper sharks (76%) were within 100 km of release locations, 16% were within 100-250 km and 8% were within 250-500 km. The most striking behavioural feature was their extensive, nearly continuous vertical movements. Median daily depth range was 184 m; the most time (61%) was spent between 150 and 450 m, but ascents above 100 m were common (58% of days). Median vertical movement rate was 6 km day(-1) and steady. The longest period of continuous vertical movement (> 60 m h(-1)) was 330 h. Systematic vertical oscillations were most common (60%), followed by diet vertical migrations (25%) and irregular vertical movements (15%). The Pacific sleeper sharks travelled below the photic zone during the day and approached the surface at night. Pacific sleeper sharks appear to employ a stealth and ambush hunting strategy that incorporates slow vertical oscillations to search for prey, and cryptic colouration and cover of darkness to avoid detection by potential prey. The depth and geographic range of Pacific sleeper shark and Steller sea lions overlap near four important Steller sea lion rookeries in the northern Gulf of Alaska, so the potential exists for predation to occur. None of the tissues in the stomachs of the 198 Pacific sleeper sharks collected during a companion diet study, however, were identified as Steller sea lion. 0 2006 The Fisheries Society of the British Isles (No claim to original US government works) C1 Natl Marine Fisheries Serv, Auke Bay Lab, Juneau, AK 99801 USA. RP Hulbert, LB (reprint author), Alaska Dept Fish & Game, Commercial Fisheries Div, POB 115526,1255 W 8th St, Juneau, AK 99811 USA. EM Lee_Hulbert@fishgame.state.ak.us NR 33 TC 32 Z9 37 U1 4 U2 29 PU BLACKWELL PUBLISHING PI OXFORD PA 9600 GARSINGTON RD, OXFORD OX4 2DQ, OXON, ENGLAND SN 0022-1112 J9 J FISH BIOL JI J. Fish Biol. PD AUG PY 2006 VL 69 IS 2 BP 406 EP 425 DI 10.1111/j.1095-8649.2006.01175.x PG 20 WC Fisheries; Marine & Freshwater Biology SC Fisheries; Marine & Freshwater Biology GA 076MF UT WOS:000239961700006 ER PT J AU Dukhan, N Picon-Feliciano, R Alvarez-Hernandez, AR AF Dukhan, Nihad Picon-Feliciano, Ruben Alvarez-Hernandez, Angel R. TI Heat transfer analysis in metal foams with low-conductivity fluids SO JOURNAL OF HEAT TRANSFER-TRANSACTIONS OF THE ASME LA English DT Article DE convection; heat transfer; porous media; metal foam ID EFFECTIVE THERMAL-CONDUCTIVITY; POROUS-MEDIA; FORCED-CONVECTION; BOUNDARY-CONDITIONS; VARIABLE POROSITY; NON-DARCIAN; FLOW; NONEQUILIBRIUM; EQUILIBRIUM; DISPERSION AB The use of open-cell metal foam in contemporary technologies is increasing rapidly. Certain simplifying assumptions for the combined conduction/convection heat transfer analysis in metal foam have not been exploited. Solving the complete, and coupled, fluid flow and heat transfer governing equations numerically is time, consuming. A simplified analytical model for the heat transfer in open-cell metal foam cooled by a low-conductivity fluid is presented. The model assumes local thermal equilibrium between the solid and fluid phases in the foam, and neglects the conduction in the fluid. The local thermal equilibrium assumption is supported by previous studies performed by other workers. The velocity profile in the foam is taken as non-Darcean slug flow. An approximate solution for the temperature profile in the foam is obtained using a similarity transform. The solution for the temperature profile is represented by the error function, which decays in what looks like an exponential fashion as the distance from the heat base increases. The model along with the simplifying assumptions were verified by direct experiment using air and several aluminum foam samples heated from below, for a range of Reynolds numbers and pore densities. The foam samples were either 5.08- or 20.32-cm-thick in the flow direction. Reasonably good agreement was found between the analytical and the experimental results for a considerable range of Reynolds numbers, with the agreement being generally C1 Univ Detroit, Dept Mech Engn, Detroit, MI 48221 USA. Univ Puerto Rico, Dept Mech Engn, Mayaguez, PR 00681 USA. NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. RP Dukhan, N (reprint author), Univ Detroit, Dept Mech Engn, 4001 W McNichols Rd, Detroit, MI 48221 USA. EM nihad.dukhan@udmercy.edu NR 44 TC 24 Z9 24 U1 0 U2 9 PU ASME PI NEW YORK PA TWO PARK AVE, NEW YORK, NY 10016-5990 USA SN 0022-1481 EI 1528-8943 J9 J HEAT TRANS-T ASME JI J. Heat Transf.-Trans. ASME PD AUG PY 2006 VL 128 IS 8 BP 784 EP 792 DI 10.1115/1.2217750 PG 9 WC Thermodynamics; Engineering, Mechanical SC Thermodynamics; Engineering GA 077EF UT WOS:000240009900012 ER PT J AU Koster, RD Guo, ZC Dirmeyer, PA Bonan, G Chan, E Cox, P Davies, H Gordon, CT Kanae, S Kowalczyk, E Lawrence, D Liu, P Lu, CH Malyshev, S McAvaney, B Mitchell, K Mocko, D Oki, T Oleson, KW Pitman, A Sud, YC Taylor, CM Verseghy, D Vasic, R Xue, YK Yamada, T AF Koster, Randal D. Guo, Zhichang Dirmeyer, Paul A. Bonan, Gordon Chan, Edmond Cox, Peter Davies, Harvey Gordon, C. T. Kanae, Shinjiro Kowalczyk, Eva Lawrence, David Liu, Ping Lu, Cheng-Hsuan Malyshev, Sergey McAvaney, Bryant Mitchell, Ken Mocko, David Oki, Taikan Oleson, Keith W. Pitman, Andrew Sud, Y. C. Taylor, Christopher M. Verseghy, Diana Vasic, Ratko Xue, Yongkang Yamada, Tomohito TI GLACE: The Global Land-Atmosphere Coupling Experiment. Part I: Overview SO JOURNAL OF HYDROMETEOROLOGY LA English DT Article ID GENERAL-CIRCULATION MODEL; ENERGY BALANCE COMPLEXITY; SCHUBERT SCHEME MCRAS; SURFACE SCHEME; SOIL-MOISTURE; TROPICAL DEFORESTATION; CLIMATE MODEL; PRECIPITATION; GCM; SIMULATIONS AB The Global Land-Atmosphere Coupling Experiment ( GLACE) is a model intercomparison study focusing on a typically neglected yet critical element of numerical weather and climate modeling: land atmosphere coupling strength, or the degree to which anomalies in land surface state ( e. g., soil moisture) can affect rainfall generation and other atmospheric processes. The 12 AGCM groups participating in GLACE performed a series of simple numerical experiments that allow the objective quantification of this element for boreal summer. The derived coupling strengths vary widely. Some similarity, however, is found in the spatial patterns generated by the models, with enough similarity to pinpoint multimodel "hot spots" of land-atmosphere coupling. For boreal summer, such hot spots for precipitation and temperature are found over large regions of Africa, central North America, and India; a hot spot for temperature is also found over eastern China. The design of the GLACE simulations are described in full detail so that any interested modeling group can repeat them easily and thereby place their model's coupling strength within the broad range of those documented here. C1 NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Ctr Ocean Land Atmosphere Studies, Calverton, MD USA. Natl Ctr Atmospher Res, Boulder, CO 80307 USA. Meteorol Serv Canada, Toronto, ON, Canada. Ctr Ecol & Hydrol, Dorset, England. CSIRO, Atmospher Res, Aspendale, Vic 3195, Australia. Geophys Fluid Dynam Lab, Princeton, NJ USA. Res Inst Human & Nat, Kyoto, Japan. Univ Reading, Reading, Berks, England. Sci Applicat Int Corp, Beltsville, MD USA. Natl Ctr Environm Predict, Camp Springs, MD USA. Princeton Univ, Princeton, NJ 08544 USA. Bur Meteorol Res Ctr, Melbourne, Vic, Australia. Univ Tokyo, Tokyo, Japan. Macquarie Univ, N Ryde, NSW, Australia. Ctr Ecol & Hydrol, Wallingford, Oxon, England. Univ Calif Los Angeles, Los Angeles, CA 90024 USA. RP Koster, RD (reprint author), NASA, Goddard Space Flight Ctr, Code 610-1, Greenbelt, MD 20771 USA. EM randal.d.koster@nasa.gov RI Oleson, Keith/A-9328-2008; Oki, Taikan/E-5778-2010; Lawrence, David/C-4026-2011; Pitman, Andrew/A-7353-2011; Koster, Randal/F-5881-2012; Taylor, Chris/K-2319-2012; Kanae, Shinjiro/E-5606-2010; Dirmeyer, Paul/B-6553-2016; Cox, Peter/B-3299-2012 OI Oki, Taikan/0000-0003-4067-4678; Lawrence, David/0000-0002-2968-3023; Pitman, Andrew/0000-0003-0604-3274; Koster, Randal/0000-0001-6418-6383; Taylor, Chris/0000-0002-0120-3198; Kanae, Shinjiro/0000-0002-3176-4957; Dirmeyer, Paul/0000-0003-3158-1752; NR 57 TC 302 Z9 303 U1 7 U2 61 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 1525-755X EI 1525-7541 J9 J HYDROMETEOROL JI J. Hydrometeorol. PD AUG PY 2006 VL 7 IS 4 BP 590 EP 610 DI 10.1175/JHM510.1 PG 21 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 086DO UT WOS:000240653900002 ER PT J AU Guo, ZC Dirmeyer, PA Koster, RD Bonan, G Chan, E Cox, P Gordon, CT Kanae, S Kowalczyk, E Lawrence, D Liu, P Lu, CH Malyshev, S McAvaney, B McGregor, JL Mitchell, K Mocko, D Oki, T Oleson, KW Pitman, A Sud, YC Taylor, CM Verseghy, D Vasic, R Xue, YK Yamada, T AF Guo, Zhichang Dirmeyer, Paul A. Koster, Randal D. Bonan, Gordon Chan, Edmond Cox, Peter Gordon, C. T. Kanae, Shinjiro Kowalczyk, Eva Lawrence, David Liu, Ping Lu, Cheng-Hsuan Malyshev, Sergey McAvaney, Bryant McGregor, J. L. Mitchell, Ken Mocko, David Oki, Taikan Oleson, Keith W. Pitman, Andrew Sud, Y. C. Taylor, Christopher M. Verseghy, Diana Vasic, Ratko Xue, Yongkang Yamada, Tomohito TI GLACE: The Global Land-Atmosphere Coupling Experiment. Part II: Analysis SO JOURNAL OF HYDROMETEOROLOGY LA English DT Article ID GENERAL-CIRCULATION MODELS; SOIL-MOISTURE; SURFACE SCHEMES; BOUNDARY-LAYER; ANNUAL CYCLE; CLIMATE; VARIABILITY; VEGETATION; GCM AB The 12 weather and climate models participating in the Global Land-Atmosphere Coupling Experiment ( GLACE) show both a wide variation in the strength of land-atmosphere coupling and some intriguing commonalities. In this paper, the causes of variations in coupling strength-both the geographic variations within a given model and the model-to-model differences-are addressed. The ability of soil moisture to affect precipitation is examined in two stages, namely, the ability of the soil moisture to affect evaporation, and the ability of evaporation to affect precipitation. Most of the differences between the models and within a given model are found to be associated with the first stage-an evaporation rate that varies strongly and consistently with soil moisture tends to lead to a higher coupling strength. The first-stage differences reflect identifiable differences in model parameterization and model climate. Intermodel differences in the evaporation-precipitation connection, however, also play a key role. C1 Ctr Ocean Land Atmosphere Studies, Calverton, MD 20705 USA. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Natl Ctr Atmospher Res, Boulder, CO 80307 USA. Meteorol Serv Canada, Toronto, ON, Canada. Ctr Ecol & Hydrol, Dorset, England. Geophys Fluid Dynam Lab, Princeton, NJ USA. Res Inst Human & Nat, Kyoto, Japan. CSIRO, Atmosphere Res, Aspendale, Vic, Australia. Univ Reading, Reading, Berks, England. Sci Applicat Int Corp, Beltsville, MD USA. Natl Ctr Environm Predict, Camp Springs, MD USA. Princeton Univ, Princeton, NJ 08544 USA. Bur Meteorol, Res Ctr, Melbourne, Vic, Australia. Univ Tokyo, Tokyo, Japan. Macquarie Univ, N Ryde, NSW, Australia. Ctr Ecol & Hydrol, Wallingford, Oxon, England. Univ Calif Los Angeles, Los Angeles, CA 90024 USA. RP Guo, ZC (reprint author), Ctr Ocean Land Atmosphere Studies, 4041 Powder Mill Rd,Suite 302, Calverton, MD 20705 USA. EM guo@cola.iges.org RI Oleson, Keith/A-9328-2008; Oki, Taikan/E-5778-2010; Lawrence, David/C-4026-2011; Pitman, Andrew/A-7353-2011; McGregor, John/C-6646-2012; Koster, Randal/F-5881-2012; Taylor, Chris/K-2319-2012; Kanae, Shinjiro/E-5606-2010; Dirmeyer, Paul/B-6553-2016; Cox, Peter/B-3299-2012 OI Oki, Taikan/0000-0003-4067-4678; Lawrence, David/0000-0002-2968-3023; Pitman, Andrew/0000-0003-0604-3274; Koster, Randal/0000-0001-6418-6383; Taylor, Chris/0000-0002-0120-3198; Kanae, Shinjiro/0000-0002-3176-4957; Dirmeyer, Paul/0000-0003-3158-1752; NR 19 TC 178 Z9 180 U1 1 U2 35 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 AUG PY 2006 VL 7 IS 4 BP 611 EP 625 DI 10.1175/JHM511.1 PG 15 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 086DO UT WOS:000240653900003 ER PT J AU Butler, RAH Sagui, L Kleiner, I Brown, LR AF Butler, R. A. H. Sagui, L. Kleiner, I. Brown, L. R. TI The absorption spectrum of phosphine (PH3) between 2.8 and 3.7 mu m: Line positions, intensities, and assignments SO JOURNAL OF MOLECULAR SPECTROSCOPY LA English DT Article DE phosphine; PH3; 3 mu m bands; positions; intensities; near infrared; assignments; line parameters ID MOLECULAR SPECTROSCOPIC DATABASE; INFRARED-SPECTRUM; NU(4) BANDS; V(4) BANDS; SATURN; COEFFICIENTS; HELIUM; NU(2); NH3; CO AB Over 8000 line positions and intensities of phosphine (PH3) at 3 mu m have been measured at 0.0115 cm(-1) resolution with the McMath-Pierce Fourier Transform spectrometer at Kitt Peak. The observed line intensities ranged from 4.13 x 10(-6) to 4.69 x 10(-2) cm(-2) atm(-1) at 296 K, for line positions between 2724.477 and 3601.652 cm(-1). This region spans eight interacting vibrational states: 3v(2) (2940.8 cm(-1)), 2v(2) + v(4) (3085.6 cm(-1)), v(2) + 2v(4) (3214.9 cm(-1)), v(1) + v(2) (3307.6 cm(-1)), v(2) + v(3) (3310.5 cm(-1)), 3v(4) (similar to 3345 cm(-1)), v(1) + v(4) (3426.9 cm(-1)), and v(3) + v(4) (3432.9 cm(-1)). Assignments have been determined for all the bands except 3v(4) (a weak band in a highly congested area) for a total of 4232 transitions. The total integrated intensity for this region is 5.70 cm(-2) atm(-1) near 296 K, and assigned lines account for 79% of the observed absorption. The two strongest bands in the region are v(1) + v(4) and v(3) + v(4) with band strengths at 296 K of 1.61 and 2.01 cm(-2) atm(-1), respectively. An empirical database of PH3 line parameters (positions, intensities, and assignments) is now available. Lower state energies (corresponding to assignments from this study) and line widths from the literature are included; default values are used for unassigned features. (c) 2006 Elsevier Inc. All rights reserved. C1 Pittsburg State Univ, Pittsburg, KS 66762 USA. Univ Paris 07, CNRS, Lab Interuniv Syst Atmospher, F-94010 Creteil, France. Univ Paris 12, F-94010 Creteil, France. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Butler, RAH (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM rbutler@pittstate.edu NR 38 TC 19 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 0022-2852 J9 J MOL SPECTROSC JI J. Mol. Spectrosc. PD AUG PY 2006 VL 238 IS 2 BP 178 EP 192 DI 10.1016/j.jms.2006.04.021 PG 15 WC Physics, Atomic, Molecular & Chemical; Spectroscopy SC Physics; Spectroscopy GA 070RE UT WOS:000239540400005 ER PT J AU Makeevt, MA AF Makeevt, Maxim A. TI Self-organized quantum dot superstructures for nanoelectronic and optoelectronic applications SO JOURNAL OF NANOELECTRONICS AND OPTOELECTRONICS LA English DT Review ID ATOM MOLECULAR-DYNAMICS; ASSEMBLED GE DOTS; INAS/GAAS SQUARE NANOMESAS; SIZE-REDUCING EPITAXY; BEAM EPITAXY; INFRARED PHOTODETECTORS; ATOMISTIC SIMULATION; PARALLEL COMPUTERS; STRESS-RELAXATION; STRAIN PROFILES AB In the last decade, a significant progress has been made towards development of new conceptual paradigms for integrating the nano-structured materials into novel electronic and optoelectronic devices. The systems of nanostructures of interest include, but not limited to, arrays of clusters, nanoparticles, quantum dots and wires, and carbon nanotubes. For a number of potential applications the systems of nanostructures must be ordered and highly homogeneous in size in order to exploit the quantum effects for device applications. In this work, a review of the recent advances in understanding the self-assembly of quantum dots grown on non-planar (patterned) substrates is given. The main emphasis is put on the mechanism of formation of highly ordered arrays of Ge/Si(001) and InAs/GaAs quantum dots taking place during growth on non-planar (patterned) substrates. C1 Univ So Calif, Dept Mat Sci & Engn, Collaboratory Adv Comp & Simulat, Los Angeles, CA 90089 USA. RP Makeevt, MA (reprint author), NASA, Ames Res Ctr, Mail Stop 229-1, Moffett Field, CA 94035 USA. NR 90 TC 4 Z9 4 U1 4 U2 27 PU AMER SCIENTIFIC PUBLISHERS PI VALENCIA PA 26650 THE OLD RD, STE 208, VALENCIA, CA 91381-0751 USA SN 1555-130X J9 J NANOELECTRON OPTOE JI J. Nanoelectron. Optoelectron. PD AUG PY 2006 VL 1 IS 2 BP 176 EP 193 DI 10.1166/jno.2006.203 PG 18 WC Engineering, Electrical & Electronic; Nanoscience & Nanotechnology; Physics, Applied SC Engineering; Science & Technology - Other Topics; Physics GA 191EF UT WOS:000248112200002 ER PT J AU Clayton, LM Gerasimov, TG Cinke, M Meyyappan, M Harmon, JP AF Clayton, LaNetra M. Gerasimov, Timofey G. Cinke, Martin Meyyappan, M. Harmon, Julie P. TI Dispersion of single-walled carbon nanotubes in a non-polar polymer, poly(4-methyl-1-pentene) SO JOURNAL OF NANOSCIENCE AND NANOTECHNOLOGY LA English DT Article DE poly(4-methyl-pentene); radiation shielding material; Galactic Cosmic Radiation; nanocomposites; polymer carbon nanotube composites ID NANOTUBE/POLY(METHYL METHACRYLATE) COMPOSITES; DYNAMIC-MECHANICAL BEHAVIOR; NANOCOMPOSITES; POLY-4-METHYLPENTENE-1; FABRICATION; PENTENE-1); RADIATION; SENSORS AB Poly(4-methyl-1-pentene), PMP, a high melting polymer composed of hydrogen and carbon, has the potential to become an alternative to polyethylene (PE) as shielding material against Galactic Cosmic Radiation (GCR). PMP exhibits higher thermal stability than PE and is transparent in the UV/visible region of the electromagnetic spectrum. Single walled carbon nanotubes (SWNTs) were pretreated with a polar solvent, N,N-Dimethylformimide (DMF), and then dispersed in a halogenated hydrocarbon, cyclohexyl chloride, which also dissolved the non polar polymer, PMP. The composites were characterized via differential scanning calorimetry (DSC), dynamic mechanical analysis (DMA), microhardness measurements, and optical microscopy. DMA data revealed that the carbon nanotubes contributed to the enhancement of the high temperature a, relaxation which is thought to arise from motion around crystalline regions in the matrix. The storage modulus (60 Hz) increased from 2409 MPa in the neat PMP to 3716 MPa at -50 degrees C. The magnitude of the increase diminished near and above the glass transition region; the glassy matrix restricted motion of the crystalline regions. DSC data showed an increase in the percent crystallinity of the composite (75%) as compared to the neat polymer (68%). Low concentrations of nanotubes, when well dispersed, produced nanocomposites with varying degrees of transparency. C1 Univ S Florida, Dept Chem, Tampa, FL 33620 USA. NASA, Ames Res Ctr, Ctr Nanotechnol, Moffett Field, CA 94035 USA. RP Harmon, JP (reprint author), Univ S Florida, Dept Chem, 4202 E Fowler Ave, Tampa, FL 33620 USA. NR 41 TC 11 Z9 11 U1 1 U2 16 PU AMER SCIENTIFIC PUBLISHERS PI STEVENSON RANCH PA 25650 NORTH LEWIS WAY, STEVENSON RANCH, CA 91381-1439 USA SN 1533-4880 J9 J NANOSCI NANOTECHNO JI J. Nanosci. Nanotechnol. PD AUG PY 2006 VL 6 IS 8 BP 2520 EP 2524 DI 10.1166/jnn.2006.537 PG 5 WC Chemistry, Multidisciplinary; Nanoscience & Nanotechnology; Materials Science, Multidisciplinary; Physics, Applied; Physics, Condensed Matter SC Chemistry; Science & Technology - Other Topics; Materials Science; Physics GA 073ZD UT WOS:000239780500037 PM 17037866 ER PT J AU Kaur, C Sivakumar, V Ang, LS Sundaresan, A AF Kaur, Charanjit Sivakumar, Viswanathan Ang, Lin Stella Sundaresan, Alamelu TI Hypoxic damage to the periventricular white matter in neonatal brain: role of vascular endothelial growth factor, nitric oxide and excitotoxicity SO JOURNAL OF NEUROCHEMISTRY LA English DT Article DE excitotoxicity; hypoxia; neonatal brain; nitric oxide; periventricular white matter damage; vascular endothelial growth factor ID INDUCIBLE FACTOR-1; PREMATURE-INFANTS; AMEBOID MICROGLIA; O-2 HOMEOSTASIS; GENE-EXPRESSION; POSTNATAL RATS; FETAL SHEEP; LEUKOMALACIA; INJURY; BARRIER AB The present study examined factors that may be involved in the development of hypoxic periventricular white matter damage in the neonatal brain. Wistar rats (1-day old) were subjected to hypoxia and the periventricular white matter (corpus callosum) was examined for the mRNA and protein expression of hypoxia-inducible factor-1 alpha (HIF-1 alpha), endothelial, neuronal and inducible nitric oxide synthase (eNOS, nNOS and iNOS), vascular endothelial growth factor (VEGF) and N-methyl-D-aspartate receptor subunit 1 (NMDAR1) between 3 h and 14 days after hypoxic exposure by real-time RT-PCR, western blotting and immunohistochemistry. Up-regulated mRNA and protein expression of HIF-1 alpha, VEGF, NMDAR1, eNOS, nNOS and iNOS in corpus callosum was observed in response to hypoxia. NMDAR1 and iNOS expression was found in the activated microglial cells, whereas VEGF was localized to astrocytes. An enzyme immunoassay showed that the VEGF concentration in corpus callosum was significantly higher up to 7 days after hypoxic exposure. NO levels, measured by colorimetric assay, were also significantly higher in hypoxic rats up to 14 days after hypoxic exposure as compared with the controls. A large number of axons undergoing degeneration were observed between 3 h and 7 days after the hypoxic exposure at electron-microscopic level. Our findings point towards the involvement of excitotoxicity, VEGF and NO in periventricular white matter damage in response to hypoxia. C1 Natl Univ Singapore, Dept Anat, Yong Loo Lin Sch Med, Singapore 117597, Singapore. Texas So Univ, Dept Biol, NASA, Houston, TX 77004 USA. RP Kaur, C (reprint author), Natl Univ Singapore, Dept Anat, Yong Loo Lin Sch Med, Blk MD10,4 Med Dr, Singapore 117597, Singapore. EM antkaurc@nus.edu.sg NR 51 TC 72 Z9 76 U1 2 U2 13 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0022-3042 EI 1471-4159 J9 J NEUROCHEM JI J. Neurochem. PD AUG PY 2006 VL 98 IS 4 BP 1200 EP 1216 DI 10.1111/j.1471-4159.2006.03964.x PG 17 WC Biochemistry & Molecular Biology; Neurosciences SC Biochemistry & Molecular Biology; Neurosciences & Neurology GA 067MM UT WOS:000239307200019 PM 16787408 ER PT J AU Shebalin, JV AF Shebalin, John V. TI Ideal homogeneous magnetohydrodynamic turbulence in the presence of rotation and a mean magnetic field SO JOURNAL OF PLASMA PHYSICS LA English DT Article ID ABSOLUTE EQUILIBRIUM; BROKEN ERGODICITY AB The statistical theory of absolute equilibrium ensembles is extended to describe ideal, three-dimensional, magnetohydrodynamic (MHD) turbulence with and without rotation, and with and without a. mean magnetic field. Results from seven long-time numerical simulations of five general eases on a 32(3) grid are presented. One notable result is the discovery of a new ideal invariant, the 'parallel helicity,' which arises when rotation and mean magnetic field vectors are aligned. Although the basic equations and statistical theory are symmetric under parity or charge reversal, the presence of invariant cross, magnetic or parallel helicity dynamically breaks this symmetry. Ideal MHD turbulence is, in general, nonergodic due to the decomposability of the constant energy surface in phase space. Non-ergodicity can be manifested in the appearance of coherent structure as long as magnetic or parallel helicity is invariant. The fact that MHD turbulence inherently contains coherent structure in certain general cases may have important implications for dynamo theory. C1 NASA, Lyndon B Johnson Space Ctr, Adv Space Propuls Lab, Houston, TX 77058 USA. RP Shebalin, JV (reprint author), NASA, Lyndon B Johnson Space Ctr, Adv Space Propuls Lab, Houston, TX 77058 USA. NR 28 TC 14 Z9 14 U1 0 U2 0 PU CAMBRIDGE UNIV PRESS PI NEW YORK PA 32 AVENUE OF THE AMERICAS, NEW YORK, NY 10013-2473 USA SN 0022-3778 J9 J PLASMA PHYS JI J. Plasma Phys. PD AUG PY 2006 VL 72 BP 507 EP 524 DI 10.1017/S0022377805004228 PN 4 PG 18 WC Physics, Fluids & Plasmas SC Physics GA 068MH UT WOS:000239377800008 ER PT J AU Wang, DW Tzou, HS Arnold, SM Lee, HJ AF Wang, D. W. Tzou, H. S. Arnold, S. M. Lee, H. -J. TI Control of static shape, dynamic oscillation, and thermally induced vibration of nozzles SO JOURNAL OF PRESSURE VESSEL TECHNOLOGY-TRANSACTIONS OF THE ASME LA English DT Article ID CONICAL SHELLS; ELEMENT AB Static shape actuation and dynamic control of nozzles can improve their performance, accuracy, reliability, etc. A new curved laminated piezothermoelastic hexahedral finite element is formulated based on the layerwise constant shear angle theory and it is used for modeling and analysis of piezothermoelastic conical shell structures subjected to control voltages for static shape actuation and dynamically and thermally induced vibration controls. Free vibration characteristics of an elastic truncated conical shell nozzle with fixed-free boundary conditions are studied using the new finite element. Both frequencies and mode shapes are accurately computed and compared favorably with available experimental and other numerical data. This study is then extended to evaluate control effectiveness of the conical shell with laminated piezoelectric layers. Static shape control is achieved by an applied electric potential. Vibration sensing and control are carried out using the negative velocity control scheme. Control of thermal excitation is also investigated. Analysis data suggest that the dynamic behavior and control characteristics of conical shells are quite complicated due to the coupled membrane and bending effects participating in the responses. To improve control effectiveness, segmentation and/or shaping of sensor and actuator layers need to be further investigated. C1 Univ Kentucky, Dept Mech Engn, Structron Lab, Lexington, KY 40506 USA. NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. RP Wang, DW (reprint author), Univ Kentucky, Dept Mech Engn, Structron Lab, Lexington, KY 40506 USA. EM hstzou@engr.uky.edu NR 17 TC 0 Z9 0 U1 0 U2 7 PU ASME-AMER SOC MECHANICAL ENG PI NEW YORK PA THREE PARK AVE, NEW YORK, NY 10016-5990 USA SN 0094-9930 J9 J PRESS VESS-T ASME JI J. Press. Vessel Technol.-Trans. ASME PD AUG PY 2006 VL 128 IS 3 BP 357 EP 363 DI 10.1115/1.2217968 PG 7 WC Engineering, Mechanical SC Engineering GA 076UD UT WOS:000239982400009 ER PT J AU Condron, CL Kauzlarich, SM Gascoin, F Snyder, GJ AF Condron, Cathie L. Kauzlarich, Susan M. Gascoin, Franck Snyder, G. Jeffrey TI Thermoelectric properties and microstructure of Mg3Sb2 SO JOURNAL OF SOLID STATE CHEMISTRY LA English DT Article DE high temperature thermoelectric; calorimetry; Mg3Sb2; thermoelectric; zintl phase; zintl; composite thermoelectric; antimonide AB Mg3Sb2 has been prepared by direct reaction of the elements. Powder X-ray diffraction, thermal gravimetric, differential scanning calorimetery, and microprobe data were obtained on hot pressed samples. Single phase samples of Mg3Sb2 were prepared and found to contain oxygen at the grain boundaries and to lose Mg and oxidize at temperatures above 900K. Thermoelectric properties were characterized by Seebeck, electrical resistivity, and thermal conductivity measurements from 300 to 1023 K, and the maximum zT was found to be 0.21 at similar to 875 K. (c) 2006 Elsevier Inc. All rights reserved. C1 Univ Calif Davis, Dept Chem, Davis, CA 95616 USA. CALTECH, Pasadena, CA 91125 USA. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Kauzlarich, SM (reprint author), Univ Calif Davis, Dept Chem, 1 Shields Ave, Davis, CA 95616 USA. EM smkauzlarich@ucdavis.edu RI Snyder, G. Jeffrey/E-4453-2011; Snyder, G/I-2263-2015; Kauzlarich, Susan/H-1439-2011 OI Snyder, G. Jeffrey/0000-0003-1414-8682; NR 17 TC 39 Z9 39 U1 8 U2 23 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0022-4596 EI 1095-726X J9 J SOLID STATE CHEM JI J. Solid State Chem. PD AUG PY 2006 VL 179 IS 8 BP 2252 EP 2257 DI 10.1016/j.jssc.2006.01.034 PG 6 WC Chemistry, Inorganic & Nuclear; Chemistry, Physical SC Chemistry GA 071YK UT WOS:000239639600002 ER PT J AU Choi, DI AF Choi, Dae-Il TI Towards wave-zone extraction of gravitational waveforms in numerical relativity simulations of binary black holes SO JOURNAL OF THE KOREAN PHYSICAL SOCIETY LA English DT Article DE numerical relativity; gravitational wave; gravitation AB We present the results from numerical relativity simulations of binary black hole coalescence. Our primary motivation is to calculate gravitational waveforms that are relevant to the space-based gravitational wave detector LISA in order to address questions that can contribute to an understanding of the scientific issues that the LISA detector will study. Our methodology includes the fixed mesh refinement technique, a novel wave-zone waveform extraction technique based on a Newman-Pensore Weyl scalar, Psi(4), a combination of second- and fourth-order finite differencing, and gauge conditions that allow black holes to move across the computational grid. A combination of these tools makes it possible to accurately describe source dynamics of black holes while keeping the outer boundary sufficiently far away to allow robust and accurate extraction of gravitational waveforms in the wave-zone. We use a head-on collision as a calibration problem to validate the approach. Here, we report on the current status of the project. C1 NASA, Goddard Space Flight Ctr, Explorat & Univ Div, Greenbelt, MD 20771 USA. Univ Space Res Assoc, Columbia, MD 21044 USA. RP Choi, DI (reprint author), NASA, Goddard Space Flight Ctr, Explorat & Univ Div, Greenbelt, MD 20771 USA. EM choi@godel.gsfc.nasa.gov NR 18 TC 1 Z9 1 U1 0 U2 0 PU KOREAN PHYSICAL SOC PI SEOUL PA 635-4, YUKSAM-DONG, KANGNAM-KU, SEOUL 135-703, SOUTH KOREA SN 0374-4884 J9 J KOREAN PHYS SOC JI J. Korean Phys. Soc. PD AUG PY 2006 VL 49 IS 2 SI SI BP 835 EP 839 PN 1 PG 5 WC Physics, Multidisciplinary SC Physics GA 073IL UT WOS:000239736100024 ER PT J AU Sakaki, K Nakamura, Y Shirai, Y Bowman, RC Akiba, E AF Sakaki, Kouji Nakamura, Yumiko Shirai, Yasuharu Bowman, Robert C., Jr. Akiba, Etsuo TI Lattice defect behavior of LaNi4.97Sn0.27 during hydrogenation cycles SO MATERIALS TRANSACTIONS LA English DT Article DE hydrogen storage; lattice defects; positron lifetime ID POSITRON LIFETIME SPECTRA; ANNIHILATION; DEGRADATION; PROGRAM; SYSTEM AB Lattice defect behavior of LaNi4.97Sn0.27 during the hydrogenation cycles has been investigated by in-situ positron lifetime measurement. Mean positron lifetime increased and decreased by each hydrogenation and dehydrogenation, respectively, independently of the hydrogenation cycles. It suggests that lattice defects are introduced by the hydrogenation and removed from the lattice by the dehydrogenation even at below the migration temperature of vacancy in LaNi5. Furthermore, dislocation density and vacancy concentration kept almost constant at the value of around 6 x 10(9) cm(-2) and 10ppm through at least eight hydrogenation/dehydrogenation cycles. C1 AIST, Tsukuba, Ibaraki 3050035, Japan. Osaka Univ, Dept Mat Sci & Engn, Suita, Osaka 5650871, Japan. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Sakaki, K (reprint author), AIST, Tsukuba, Ibaraki 3050035, Japan. NR 17 TC 1 Z9 1 U1 1 U2 3 PU JAPAN INST METALS PI SENDAI PA 1-14-32, ICHIBANCHO, AOBA-KU, SENDAI, 980-8544, JAPAN SN 1345-9678 EI 1347-5320 J9 MATER TRANS JI Mater. Trans. PD AUG PY 2006 VL 47 IS 8 BP 1875 EP 1877 DI 10.2320/matertrans.47.1875 PG 3 WC Materials Science, Multidisciplinary; Metallurgy & Metallurgical Engineering SC Materials Science; Metallurgy & Metallurgical Engineering GA 093FG UT WOS:000241152800001 ER PT J AU Abell, PA Mittlefehldt, DW Gaffey, MJ AF Abell, P. A. Mittlefehldt, D. W. Gaffey, M. J. TI Characterization of asteroidal basalts through reflectance spectroscopy and implications for the Dawn mission SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 69th Annual Meeting of the Meteoritical Society CY AUG 06-11, 2006 CL Zurich, SWITZERLAND SP Meteorit Soc, ETH Zurich, Swiss Natl Sci Fdn, Swiss Acad Nat Sci, Lunar & Planetary Inst, Barringer Crater Co, Meteorite Magazine, Planetary Studies Fdn, Jungfrau Railway Top Europe ID VESTA; SPACE C1 NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. Univ N Dakota, Dept Space Studies, Grand Forks, ND 58202 USA. 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 AUG PY 2006 VL 41 IS 8 SU S BP A13 EP A13 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 065PR UT WOS:000239172300006 ER PT J AU Barakat, AA Sculte, M AF Barakat, Aly A. Sculte, Mitch TI The meteorite of Minqar Abd el Nabi, western desert, Egypt SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 69th Annual Meeting of the Meteoritical Society CY AUG 06-11, 2006 CL Zurich, SWITZERLAND SP Meteorit Soc, ETH Zurich, Swiss Natl Sci Fdn, Swiss Acad Nat Sci, Lunar & Planetary Inst, Barringer Crater Co, Meteorite Magazine, Planetary Studies Fdn, Jungfrau Railway Top Europe C1 Egyptian Mineral Resource Author, Cairo, Egypt. NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. NR 5 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 AUG PY 2006 VL 41 IS 8 SU S BP A201 EP A201 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 065PR UT WOS:000239172300380 ER PT J AU Botta, O Martins, Z Emmenegger, C Dworkin, JP Glavin, DP Harvey, RP Zenobi, R Ehrenfreund, P AF Botta, O. Martins, Z. Emmenegger, C. Dworkin, J. P. Glavin, D. P. Harvey, R. P. Zenobi, R. Ehrenfreund, P. TI Amino acids and polycyclic aromatic hydrocarbons in meteorites and ice samples from La Paz ice field, Antarctica SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 69th Annual Meeting of the Meteoritical Society CY AUG 06-11, 2006 CL Zurich, SWITZERLAND SP Meteorit Soc, ETH Zurich, Swiss Natl Sci Fdn, Swiss Acad Nat Sci, Lunar & Planetary Inst, Barringer Crater Co, Meteorite Magazine, Planetary Studies Fdn, Jungfrau Railway Top Europe ID MASS-SPECTROMETRY C1 NASA, Goddard Ctr Astrobiol, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Leiden Univ, Leiden Inst Chem, Astrobiol Lab, NL-2300 RA Leiden, Netherlands. ETHZ Honggerberg, Dept Chem & Appl Biosci, CH-8093 Zurich, Switzerland. Case Western Reserve Univ, Dept Geol, Cleveland, OH 44106 USA. EM Oliver.Botta.1@gsfc.nasa.gov RI Zenobi, Renato/F-1113-2010; Glavin, Daniel/D-6194-2012; Dworkin, Jason/C-9417-2012 OI Glavin, Daniel/0000-0001-7779-7765; Dworkin, Jason/0000-0002-3961-8997 NR 3 TC 2 Z9 2 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 AUG PY 2006 VL 41 IS 8 SU S BP A26 EP A26 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 065PR UT WOS:000239172300032 ER PT J AU Chizmadia, LJ Nuth, JA AF Chizmadia, L. J. Nuth, J. A., III TI Kinetics of phyllosilicate formation in hydrated magnesiosilicate smokes SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 69th Annual Meeting of the Meteoritical Society CY AUG 06-11, 2006 CL Zurich, SWITZERLAND SP Meteorit Soc, ETH Zurich, Swiss Natl Sci Fdn, Swiss Acad Nat Sci, Lunar & Planetary Inst, Barringer Crater Co, Meteorite Magazine, Planetary Studies Fdn, Jungfrau Railway Top Europe ID CARBONACEOUS CHONDRITES; SILICATES; MATRIX C1 Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. Hawaii Inst Geophys & Planetol, Honolulu, HI 96822 USA. NASA, Astrochem Lab, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. EM lchiz@ifa.hawaii.edu NR 9 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 AUG PY 2006 VL 41 IS 8 SU S BP A37 EP A37 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 065PR UT WOS:000239172300055 ER PT J AU Downes, H Mittlefehldt, DW AF Downes, H. Mittlefehldt, D. W. TI Identification of a common R chondrite impactor on the ureilite parent body SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 69th Annual Meeting of the Meteoritical Society CY AUG 06-11, 2006 CL Zurich, SWITZERLAND SP Meteorit Soc, ETH Zurich, Swiss Natl Sci Fdn, Swiss Acad Nat Sci, Lunar & Planetary Inst, Barringer Crater Co, Meteorite Magazine, Planetary Studies Fdn, Jungfrau Railway Top Europe ID RUMURUTI; METEORITE; MEMBER C1 Birkbeck Univ London, London WC1E 7HX, England. Lunar & Planetary Inst, Houston, TX 77054 USA. NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. EM b.downes@ucl.ac.uk NR 12 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 AUG PY 2006 VL 41 IS 8 SU S BP A46 EP A46 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 065PR UT WOS:000239172300073 ER PT J AU Heber, VS Wiens, RC Olinger, C Burnett, DS Baur, H Wiechert, U Wieler, R AF Heber, V. S. Wiens, R. C. Olinger, C. Burnett, D. S. Baur, H. Wiechert, U. Wieler, R. TI Mass-fractionation induced by the Genesis solar wind concentrator: Analysis of neon isotopes by UV laser ablation SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 69th Annual Meeting of the Meteoritical Society CY AUG 06-11, 2006 CL Zurich, SWITZERLAND SP Meteorit Soc, ETH Zurich, Swiss Natl Sci Fdn, Swiss Acad Nat Sci, Lunar & Planetary Inst, Barringer Crater Co, Meteorite Magazine, Planetary Studies Fdn, Jungfrau Railway Top Europe C1 ETH, Isotope Geol, CH-8092 Zurich, Switzerland. LANL, Space & Atmospher Sci, Los Alamos, NM 87544 USA. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. FU Berlin, AG Geochem, D-12249 Berlin, Germany. EM heber@erdw.ethz.ch RI Wieler, Rainer/A-1355-2010 OI Wieler, Rainer/0000-0001-5666-7494 NR 3 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 AUG PY 2006 VL 41 IS 8 SU S BP A72 EP A72 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 065PR UT WOS:000239172300125 ER PT J AU Herrin, JS Mittlefehldt, DW Humayun, M AF Herrin, J. S. Mittlefehldt, D. W. Humayun, M. TI History of metal veins in acapulcoite-lodranite clan meteorite GRA 95209 SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 69th Annual Meeting of the Meteoritical Society CY AUG 06-11, 2006 CL Zurich, SWITZERLAND SP Meteorit Soc, ETH Zurich, Swiss Natl Sci Fdn, Swiss Acad Nat Sci, Lunar & Planetary Inst, Barringer Crater Co, Meteorite Magazine, Planetary Studies Fdn, Jungfrau Railway Top Europe C1 NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. Florida State Univ, Dept Geol Sci, Tallahassee, FL 32306 USA. Florida State Univ, Natl High Magnet Field Lab, Tallahassee, FL 32306 USA. EM jason.s.herrin1@jsc.nasa.gov NR 4 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 AUG PY 2006 VL 41 IS 8 SU S BP A75 EP A75 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 065PR UT WOS:000239172300130 ER PT J AU Kearsley, AT Burchell, MJ Wozniakiewicz, P Cole, MJ Graham, GA Chater, RJ Dai, Z Teslich, N Horz, F Schwandt, C AF Kearsley, A. T. Burchell, M. J. Wozniakiewicz, P. Cole, M. J. Graham, G. A. Chater, R. J. Dai, Z. Teslich, N. Horz, F. Schwandt, C. TI Calibration for Stardust craters in aluminum foil: Interpretation of cometary particle properties by comparison with laboratory impacts of mineral, polymer, and glass grains SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 69th Annual Meeting of the Meteoritical Society CY AUG 06-11, 2006 CL Zurich, SWITZERLAND SP Meteorit Soc, ETH Zurich, Swiss Natl Sci Fdn, Swiss Acad Nat Sci, Lunar & Planetary Inst, Barringer Crater Co, Meteorite Magazine, Planetary Studies Fdn, Jungfrau Railway Top Europe ID HYPERVELOCITY IMPACT C1 Nat Hist Museum, London SW7 5BD, England. Univ Kent, Canterbury CT2 7NH, Kent, England. LLNL, Livermore, CA 94550 USA. Univ London Imperial Coll Sci Technol & Med, London SW7 2BP, England. NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. NR 5 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 AUG PY 2006 VL 41 IS 8 SU S BP A92 EP A92 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 065PR UT WOS:000239172300165 ER PT J AU Kimura, Y Nuth, JA AF Kimura, Y. Nuth, J. A., III TI Variety of refractory oxide grains depend on formation environments SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 69th Annual Meeting of the Meteoritical Society CY AUG 06-11, 2006 CL Zurich, SWITZERLAND SP Meteorit Soc, ETH Zurich, Swiss Natl Sci Fdn, Swiss Acad Nat Sci, Lunar & Planetary Inst, Barringer Crater Co, Meteorite Magazine, Planetary Studies Fdn, Jungfrau Railway Top Europe ID PARTICLES; CONDENSATION; IRON C1 Ritsumeikan Univ, Kyoto, Japan. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. EM ykimura@se.ritsumei.ac.jp RI Kimura, Yuki/J-9635-2014 OI Kimura, Yuki/0000-0002-9218-7663 NR 8 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 AUG PY 2006 VL 41 IS 8 SU S BP A95 EP A95 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 065PR UT WOS:000239172300171 ER PT J AU Kletetschka, G Wasilewski, PJ Kohout, T Adachi, T Mikula, V AF Kletetschka, G. Wasilewski, P. J. Kohout, T. Adachi, T. Mikula, V. TI Protocol for first order paleofields estimation SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 69th Annual Meeting of the Meteoritical Society CY AUG 06-11, 2006 CL Zurich, SWITZERLAND SP Meteorit Soc, ETH Zurich, Swiss Natl Sci Fdn, Swiss Acad Nat Sci, Lunar & Planetary Inst, Barringer Crater Co, Meteorite Magazine, Planetary Studies Fdn, Jungfrau Railway Top Europe C1 Catholic Univ Amer, Washington, DC 20064 USA. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Acad Sci Czech Republ, Prague, Czech Republic. Charles Univ, Prague, Czech Republic. Univ Helsinki, Helsinki, Finland. EM Kletetschka@gsfc.nasa.gov RI Kohout, Tomas/C-1394-2008; Kletetschka, Gunther/C-9996-2011 OI Kohout, Tomas/0000-0003-4458-3650; Kletetschka, Gunther/0000-0002-0645-9037 NR 0 TC 0 Z9 0 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 AUG PY 2006 VL 41 IS 8 SU S BP A97 EP A97 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 065PR UT WOS:000239172300175 ER PT J AU Leitner, J Stephan, T Kearsley, AT Horz, F AF Leitner, J. Stephan, T. Kearsley, A. T. Hoerz, F. TI TOF-SIMS analysis of crater residues from projectiles shot onto aluminum foil SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 69th Annual Meeting of the Meteoritical Society CY AUG 06-11, 2006 CL Zurich, SWITZERLAND SP Meteorit Soc, ETH Zurich, Swiss Natl Sci Fdn, Swiss Acad Nat Sci, Lunar & Planetary Inst, Barringer Crater Co, Meteorite Magazine, Planetary Studies Fdn, Jungfrau Railway Top Europe C1 Inst Planetol, D-48149 Munster, Germany. Nat Hist Museum, London SW7 5BD, England. NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. EM leitner@uni-muenster.de RI Leitner, Jan/A-7391-2015 OI Leitner, Jan/0000-0003-3655-6273 NR 8 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 AUG PY 2006 VL 41 IS 8 SU S BP A105 EP A105 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 065PR UT WOS:000239172300190 ER PT J AU Mabry, JC Meshik, AP Hohenberg, CM Marrocchi, Y Pravdivtseva, OV Allton, J Bastien, R McNamara, K Stansbery, E Burnett, D AF Mabry, J. C. Meshik, A. P. Hohenberg, C. M. Marrocchi, Y. Pravdivtseva, O. V. Allton, J. Bastien, R. McNamara, K. Stansbery, E. Burnett, D. TI Argon and neon in genesis aluminum-coated sapphire collectors from regime arrays SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 69th Annual Meeting of the Meteoritical Society CY AUG 06-11, 2006 CL Zurich, SWITZERLAND SP Meteorit Soc, ETH Zurich, Swiss Natl Sci Fdn, Swiss Acad Nat Sci, Lunar & Planetary Inst, Barringer Crater Co, Meteorite Magazine, Planetary Studies Fdn, Jungfrau Railway Top Europe C1 Washington Univ, Dept Phys, St Louis, MO 63130 USA. NASA, Lyndon B Johnson Space Ctr, Lockheed Martin, Houston, TX 77058 USA. CALTECH, Pasadena, CA 91125 USA. EM jcmabry@wustl.edu NR 3 TC 1 Z9 1 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 AUG PY 2006 VL 41 IS 8 SU S BP A109 EP A109 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 065PR UT WOS:000239172300199 ER PT J AU Malavergne, V Berthet, S Righter, K AF Malavergne, V. Berthet, S. Righter, K. TI CaS formation from a Cl composition at high pressure and temperature under low oxygen fugacity SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 69th Annual Meeting of the Meteoritical Society CY AUG 06-11, 2006 CL Zurich, SWITZERLAND SP Meteorit Soc, ETH Zurich, Swiss Natl Sci Fdn, Swiss Acad Nat Sci, Lunar & Planetary Inst, Barringer Crater Co, Meteorite Magazine, Planetary Studies Fdn, Jungfrau Railway Top Europe ID ENSTATITE METEORITES C1 Lunar & Planetary Inst, Houston, TX 77058 USA. Univ Marne La Vallee, Lab Geomat, F-77454 Champs Sur Marne, France. NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. EM malavergne@lpi.usra.edu NR 5 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 AUG PY 2006 VL 41 IS 8 SU S BP A111 EP A111 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 065PR UT WOS:000239172300202 ER PT J AU Martins, Z Botta, O Fogel, ML Sephton, MA Glavin, DP Watson, JS Dworkin, JP Schwartz, AW Ehrenfreund, P AF Martins, Z. Botta, O. Fogel, M. L. Sephton, M. A. Glavin, D. P. Watson, J. S. Dworkin, J. P. Schwartz, A. W. Ehrenfreund, P. TI Isotopic analysis of nucleobases in the Murchison meteorite SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 69th Annual Meeting of the Meteoritical Society CY AUG 06-11, 2006 CL Zurich, SWITZERLAND SP Meteorit Soc, ETH Zurich, Swiss Natl Sci Fdn, Swiss Acad Nat Sci, Lunar & Planetary Inst, Barringer Crater Co, Meteorite Magazine, Planetary Studies Fdn, Jungfrau Railway Top Europe ID HETEROCYCLIC COMPOUNDS C1 Leiden Univ, Leiden Inst Chem, Astrobiol Lab, NL-2300 RA Leiden, Netherlands. NASA, Goddard Space Flight Ctr, Goddard Ctr Astrobiol, Greenbelt, MD 20771 USA. Carnegie Inst Washington, Geophys Lab, Washington, DC 20015 USA. Univ London Imperial Coll Sci Technol & Med, Dept Earth Sci & Engn, Impacts & Astromat Res Ctr, London, England. Open Univ, Planetary & Space Sci Res Inst, Milton Keynes MK7 6AA, Bucks, England. Radboud Univ Nijmegen, Nijmegen, Netherlands. EM z.martins@chem.leidenuniv.nl 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 6 TC 0 Z9 0 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 AUG PY 2006 VL 41 IS 8 SU S BP A114 EP A114 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 065PR UT WOS:000239172300209 ER PT J AU McKeegan, K Aleon, J Alexander, C Bradley, J Brownlee, D Burnard, P Butterworth, A Chaussidon, M Davis, A Floss, C Gilmour, J Guan, Y Hohenberg, C Hoppe, P Hutcheon, I Ito, M Jacobsen, S Leshin, L Lyon, I Marhas, K Marty, B Meibom, A Meshik, A Messenger, S Nakamura, K Nittler, L Palma, R Pellin, M Pepin, R Tsou, P Robert, F Schlutter, D Stadermann, F Stroud, R Westphal, A Young, E Ziegler, K Zinner, E AF McKeegan, K. Aleon, J. Alexander, C. Bradley, J. Brownlee, D. Burnard, P. Butterworth, A. Chaussidon, M. Davis, A. Floss, C. Gilmour, J. Guan, Y. Hohenberg, C. Hoppe, P. Hutcheon, I. Ito, M. Jacobsen, S. Leshin, L. Lyon, I. Marhas, K. Marty, B. Meibom, A. Meshik, A. Messenger, S. Nakamura, K. Nittler, L. Palma, R. Pellin, M. Pepin, R. Tsou, P. Robert, F. Schlutter, D. Stadermann, F. Stroud, R. Westphal, A. Young, E. Ziegler, K. Zinner, E. TI Isotopic compositions of cometary matter returned by the Stardust mission SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 69th Annual Meeting of the Meteoritical Society CY AUG 06-11, 2006 CL Zurich, SWITZERLAND SP Meteorit Soc, ETH Zurich, Swiss Natl Sci Fdn, Swiss Acad Nat Sci, Lunar & Planetary Inst, Barringer Crater Co, Meteorite Magazine, Planetary Studies Fdn, Jungfrau Railway Top Europe C1 Univ Calif Los Angeles, Dept Earth & Space Sci, Los Angeles, CA 90024 USA. Carnegie Inst Washington, DTM, Washington, DC 20005 USA. Univ Washington, Seattle, WA 98195 USA. Univ Calif Berkeley, Berkeley, CA 94720 USA. Univ Chicago, Chicago, IL 60637 USA. Washington Univ, St Louis, MO 63130 USA. Univ Manchester, Manchester M13 9PL, Lancs, England. CALTECH, Pasadena, CA 91125 USA. MPI, Mainz, Germany. NASA, JSC, Greenbelt, MD USA. Harvard Univ, Cambridge, MA 02138 USA. NASA, GSFC, Greenbelt, MD USA. Museum Natl Hist Nat, F-75231 Paris, France. Univ Minnesota, Minneapolis, MN 55455 USA. NASA, JPL, Greenbelt, MD USA. EM kdm@ess.ucla.edu RI Pellin, Michael/B-5897-2008; Gilmour, Jamie/G-7515-2011; Jacobsen, Stein/B-1759-2013; Hoppe, Peter/B-3032-2015; Stroud, Rhonda/C-5503-2008 OI Pellin, Michael/0000-0002-8149-9768; Hoppe, Peter/0000-0003-3681-050X; Stroud, Rhonda/0000-0001-5242-8015 NR 3 TC 1 Z9 1 U1 1 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 AUG PY 2006 VL 41 IS 8 SU S BP A119 EP A119 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 065PR UT WOS:000239172300219 ER PT J AU Meshik, A Marrocchi, Y Hohenberg, C Pravdivtseva, O Mabry, J Allton, J Bastien, R McNamara, K Stansbery, E Burnett, D AF Meshik, A. Marrocchi, Y. Hohenberg, C. Pravdivtseva, O. Mabry, J. Allton, J. Bastien, R. McNamara, K. Stansbery, E. Burnett, D. TI Solar neon released from genesis aluminum collector duriung stepped UV-laser extraction and step-wise pyrolysis SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 69th Annual Meeting of the Meteoritical Society CY AUG 06-11, 2006 CL Zurich, SWITZERLAND SP Meteorit Soc, ETH Zurich, Swiss Natl Sci Fdn, Swiss Acad Nat Sci, Lunar & Planetary Inst, Barringer Crater Co, Meteorite Magazine, Planetary Studies Fdn, Jungfrau Railway Top Europe C1 Washington Univ, St Louis, MO 63130 USA. NASA, Lockheed Martin, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. NASA, JSC, Houston, TX 77058 USA. CALTECH, Pasadena, CA 91125 USA. EM am@physics.wustl.edu NR 4 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 AUG PY 2006 VL 41 IS 8 SU S BP A121 EP A121 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 065PR UT WOS:000239172300222 ER PT J AU Mikouchi, T Mckay, G Koizumi, E AF Mikouchi, T. McKay, G. Koizumi, E. TI Post-shock cooling history of Dhofar 378 shergottite SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 69th Annual Meeting of the Meteoritical Society CY AUG 06-11, 2006 CL Zurich, SWITZERLAND SP Meteorit Soc, ETH Zurich, Swiss Natl Sci Fdn, Swiss Acad Nat Sci, Lunar & Planetary Inst, Barringer Crater Co, Meteorite Magazine, Planetary Studies Fdn, Jungfrau Railway Top Europe C1 Univ Tokyo, Dept Earth & Planetary Sci, Tokyo 1130033, Japan. NASA, KR, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. EM mikouchi@eps.s.u-tokyo.ac.jp NR 5 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 AUG PY 2006 VL 41 IS 8 SU S BP A122 EP A122 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 065PR UT WOS:000239172300224 ER PT J AU Mittlefehldt, DW Rumble, D AF Mittlefehldt, D. W. Rumble, D., III TI Geochemistry of pallasite olivines and the origin of main-group pallasites SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 69th Annual Meeting of the Meteoritical Society CY AUG 06-11, 2006 CL Zurich, SWITZERLAND SP Meteorit Soc, ETH Zurich, Swiss Natl Sci Fdn, Swiss Acad Nat Sci, Lunar & Planetary Inst, Barringer Crater Co, Meteorite Magazine, Planetary Studies Fdn, Jungfrau Railway Top Europe C1 NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. Carnegie Inst Washington, Geophys Lab, Washington, DC 20015 USA. EM david.w.mittlefehldt@nasa.gov NR 7 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 AUG PY 2006 VL 41 IS 8 SU S BP A123 EP A123 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 065PR UT WOS:000239172300226 ER PT J AU Nuth, JA Becker, L Poreda, RJ Ferguson, FT AF Nuth, Joseph A. Becker, Luann Poreda, Robert J. Ferguson, Frank T. TI Trapping noble gases in fullerenes SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 69th Annual Meeting of the Meteoritical Society CY AUG 06-11, 2006 CL Zurich, SWITZERLAND SP Meteorit Soc, ETH Zurich, Swiss Natl Sci Fdn, Swiss Acad Nat Sci, Lunar & Planetary Inst, Barringer Crater Co, Meteorite Magazine, Planetary Studies Fdn, Jungfrau Railway Top Europe ID HELIUM C1 NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Univ Calif Santa Barbara, Inst Crustal Studies, Dept Geol Sci, Santa Barbara, CA 93106 USA. Dept Earth, Rochester, NY 14627 USA. Catholic Univ Amer, Dept Chem, Washington, DC 20064 USA. EM Joseph.A.Nuth@NASA.gov RI Ferguson, Frank/C-9493-2012 NR 8 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 AUG PY 2006 VL 41 IS 8 SU S BP A134 EP A134 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 065PR UT WOS:000239172300249 ER PT J AU Nyquist, LE Shih, CY Reese, YD AF Nyquist, L. E. Shih, C. -Y. Reese, Y. D. TI Initial isotopic heterogeneities in Zagami: Evidence of a complex magmatic history SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 69th Annual Meeting of the Meteoritical Society CY AUG 06-11, 2006 CL Zurich, SWITZERLAND SP Meteorit Soc, ETH Zurich, Swiss Natl Sci Fdn, Swiss Acad Nat Sci, Lunar & Planetary Inst, Barringer Crater Co, Meteorite Magazine, Planetary Studies Fdn, Jungfrau Railway Top Europe ID PETROGENESIS; METEORITE C1 NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. ESCG Jacobs Sverdrup, Houston, TX 77058 USA. ESCG Muniz Engn, Houston, TX 77058 USA. EM laurence.e.nyquist@nasa.gov NR 7 TC 6 Z9 6 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 AUG PY 2006 VL 41 IS 8 SU S BP A135 EP A135 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 065PR UT WOS:000239172300250 ER PT J AU Park, J Bogard, DD AF Park, J. Bogard, D. D. TI Ar-Ar age of shergottite Dhofar 378: Formation or early shock event? SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 69th Annual Meeting of the Meteoritical Society CY AUG 06-11, 2006 CL Zurich, SWITZERLAND SP Meteorit Soc, ETH Zurich, Swiss Natl Sci Fdn, Swiss Acad Nat Sci, Lunar & Planetary Inst, Barringer Crater Co, Meteorite Magazine, Planetary Studies Fdn, Jungfrau Railway Top Europe C1 NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. EM jisun.park1@jsc.nasa.gov NR 4 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 AUG PY 2006 VL 41 IS 8 SU S BP A138 EP A138 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 065PR UT WOS:000239172300257 ER PT J AU Rankenburg, K Brandon, AD Neal, CR AF Rankenburg, K. Brandon, A. D. Neal, C. R. TI Formation interval of the lunar mantle from high-precision Nd-isotope measurements of six lunar basalts #5035 SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 69th Annual Meeting of the Meteoritical Society CY AUG 06-11, 2006 CL Zurich, SWITZERLAND SP Meteorit Soc, ETH Zurich, Swiss Natl Sci Fdn, Swiss Acad Nat Sci, Lunar & Planetary Inst, Barringer Crater Co, Meteorite Magazine, Planetary Studies Fdn, Jungfrau Railway Top Europe C1 NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. Univ Notre Dame, Dept Civil Engn & Geol Sci, Notre Dame, IN 46556 USA. EM neal.1@nd.edu 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 AUG PY 2006 VL 41 IS 8 SU S BP A145 EP A145 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 065PR UT WOS:000239172300271 ER PT J AU Righter, K Bussey, B AF Righter, K. Bussey, B. TI Mineralogy and petrology of the mare basalt-rich breccia MET 01210 SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 69th Annual Meeting of the Meteoritical Society CY AUG 06-11, 2006 CL Zurich, SWITZERLAND SP Meteorit Soc, ETH Zurich, Swiss Natl Sci Fdn, Swiss Acad Nat Sci, Lunar & Planetary Inst, Barringer Crater Co, Meteorite Magazine, Planetary Studies Fdn, Jungfrau Railway Top Europe C1 NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. Johns Hopkins Univ, Appl Phys Lab, Dept Space, Planetary Explorat Grp, Laurel, MD 20723 USA. EM kevin.righter-l@nasa.gov NR 6 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 AUG PY 2006 VL 41 IS 8 SU S BP A148 EP A148 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 065PR UT WOS:000239172300276 ER PT J AU Righter, K Harvey, RP Schutt, J Satterwhite, C McBride, KM Mccoy, TJ Welzenbach, L AF Righter, K. Harvey, R. P. Schutt, J. Satterwhite, C. McBride, K. M. McCoy, T. J. Welzenbach, L. TI The great diversity of planetary materials returned from the Queen Alexandra Range, Antarctica SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 69th Annual Meeting of the Meteoritical Society CY AUG 06-11, 2006 CL Zurich, SWITZERLAND SP Meteorit Soc, ETH Zurich, Swiss Natl Sci Fdn, Swiss Acad Nat Sci, Lunar & Planetary Inst, Barringer Crater Co, Meteorite Magazine, Planetary Studies Fdn, Jungfrau Railway Top Europe C1 NASA, ESCG, Jacobs Sverdrup, JSC, Houston, TX 77058 USA. Case Western Reserve Univ, Dept Geol, Cleveland, OH 44106 USA. Smithsonian Inst, Dept Mineral Sci, Washington, DC 20560 USA. EM kevin.righter-l@nasa.gov NR 7 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 AUG PY 2006 VL 41 IS 8 SU S BP A148 EP A148 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 065PR UT WOS:000239172300277 ER PT J AU Schroder, C Gellert, R Jolliff, BL Klingelhofer, G Mccoy, TJ Morris, RV Rodionov, DS de Souza, PA Yen, AS Zipfel, J AF Schroeder, C. Gellert, R. Jolliff, B. L. Klingelhoefer, G. McCoy, T. J. Morris, R. V. Rodionov, D. S. de Souza, P. A. Yen, A. S., Jr. Zipfel, J. CA Athena Sci Team TI A stony meteorite discovered by the Mars Exploration Rover Opportunity on Meridiani Planum, Mars SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 69th Annual Meeting of the Meteoritical Society CY AUG 06-11, 2006 CL Zurich, SWITZERLAND SP Meteorit Soc, ETH Zurich, Swiss Natl Sci Fdn, Swiss Acad Nat Sci, Lunar & Planetary Inst, Barringer Crater Co, Meteorite Magazine, Planetary Studies Fdn, Jungfrau Railway Top Europe C1 Univ Mainz, Inst Anorgan & Analyt Chem, D-6500 Mainz, Germany. Univ Guelph, Guelph, ON N1G 2W1, Canada. Washington Univ, St Louis, MO USA. Smithsonian Inst, Washington, DC 20560 USA. NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. CVRD Grp, Rio De Janeiro, Brazil. CALTECH, Jet Prop Lab, Pasadena, CA USA. Forschungsinst & Nat Museum Senckenberg, Frankfurt, Germany. EM schroedc@uni-mainz.de RI de Souza, Paulo/B-8961-2008; Schroder, Christian/B-3870-2009 OI de Souza, Paulo/0000-0002-0091-8925; Schroder, Christian/0000-0002-7935-6039 NR 5 TC 4 Z9 4 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 AUG PY 2006 VL 41 IS 8 SU S BP A160 EP A160 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 065PR UT WOS:000239172300300 ER PT J AU Velbel, MA Wentworth, SJ AF Velbel, M. A. Wentworth, S. J. TI Aqueous corrosion textures on weathered chain silicate surfaces as possible terrestrial analogs of pyroxene alteration in Mars meteorites SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 69th Annual Meeting of the Meteoritical Society CY AUG 06-11, 2006 CL Zurich, SWITZERLAND SP Meteorit Soc, ETH Zurich, Swiss Natl Sci Fdn, Swiss Acad Nat Sci, Lunar & Planetary Inst, Barringer Crater Co, Meteorite Magazine, Planetary Studies Fdn, Jungfrau Railway Top Europe C1 Michigan State Univ, Dept Geol Sci, E Lansing, MI 48824 USA. NASA, ESCG, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. EM Velbel@msu.edu NR 5 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 AUG PY 2006 VL 41 IS 8 SU S BP A180 EP A180 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 065PR UT WOS:000239172300341 ER PT J AU Velbel, MA Tonui, EK Zolensky, ME AF Velbel, M. A. Tonui, E. K. Zolensky, M. E. TI Whole-rock oxygen isotope compositions are unrelated to degree of aqueous alteration in CM2 chondrites SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 69th Annual Meeting of the Meteoritical Society CY AUG 06-11, 2006 CL Zurich, SWITZERLAND SP Meteorit Soc, ETH Zurich, Swiss Natl Sci Fdn, Swiss Acad Nat Sci, Lunar & Planetary Inst, Barringer Crater Co, Meteorite Magazine, Planetary Studies Fdn, Jungfrau Railway Top Europe ID CARBONACEOUS CHONDRITES C1 Michigan State Univ, Dept Geol Sci, E Lansing, MI 48824 USA. Univ Calif Los Angeles, Dept Earth & Space Sci, Los Angeles, CA 90024 USA. NASA, Astromat Res & Explorat Sci Off, Lyndon B Johnson Space Ctr, Greenbelt, MD USA. EM velbel@msu.edu NR 6 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 AUG PY 2006 VL 41 IS 8 SU S BP A181 EP A181 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 065PR UT WOS:000239172300342 ER PT J AU Zolensky, M AF Zolensky, Michael TI Proposed search for metamorphosed carbonaceous chondrites from hot desert meteorite accumulations SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 69th Annual Meeting of the Meteoritical Society CY AUG 06-11, 2006 CL Zurich, SWITZERLAND SP Meteorit Soc, ETH Zurich, Swiss Natl Sci Fdn, Swiss Acad Nat Sci, Lunar & Planetary Inst, Barringer Crater Co, Meteorite Magazine, Planetary Studies Fdn, Jungfrau Railway Top Europe C1 NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. EM michael.e.zolensky@nasa.gov NR 8 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 AUG PY 2006 VL 41 IS 8 SU S BP A216 EP A216 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 065PR UT WOS:000239172300409 ER PT J AU Zolensky, M Bland, P Bradley, J Brearley, A Brennan, S Bridges, J Brownlee, D Buttervorth, A Dai, ZR Ebel, D Genge, M Gounelle, M Graham, G Grossman, J Grossman, L Harvey, R Ishii, H Kearsley, A Keller, L Krot, A Langenhorst, F Lanzirotti, A Leroux, H Matrajt, G Messenger, K Mikouchi, T Nakamura, T Ohsumi, K Okudaira, K Perronnet, M Rietmeijer, F Simon, S Stephan, T Stroud, R Taheri, M Tomeoka, K Toppani, A Tsou, P Tsuchiyama, A Velbel, M Weber, I Weisberg, M Westphal, A Yano, H Zega, T AF Zolensky, Michael Bland, Phil Bradley, John Brearley, Adrian Brennan, Sean Bridges, John Brownlee, Donald Buttervorth, Arma Dai, Zurong Ebel, Denton Genge, Matt Gounelle, Matthieu Graham, Giles Grossman, Jeff Grossman, Lawrence Harvey, Ralph Ishii, Hope Kearsley, Anton Keller, Lindsay Krot, Alexander Langenhorst, Falko Lanzirotti, Antonio Leroux, Hugues Matrajt, Graciela Messenger, Keiko Mikouchi, Takashi Nakamura, Tomoki Ohsumi, Kazumasa Okudaira, Kyoko Perronnet, Murielle Rietmeijer, Frans Simon, Steven Stephan, Thomas Stroud, Rhonda Taheri, Mitra Tomeoka, Kazu Toppani, Alice Tsou, Peter Tsuchiyama, Akira Velbel, Michael Weber, Iris Weisberg, Mike Westphal, Andrew Yano, Hajime Zega, Thomas CA Stardust Mineralogy Petrology TI Mineralogy and petrology of Comet Wild-2 nucleus samples - Final results of the preliminary examination team SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 69th Annual Meeting of the Meteoritical Society CY AUG 06-11, 2006 CL Zurich, SWITZERLAND SP Meteorit Soc, ETH Zurich, Swiss Natl Sci Fdn, Swiss Acad Nat Sci, Lunar & Planetary Inst, Barringer Crater Co, Meteorite Magazine, Planetary Studies Fdn, Jungfrau Railway Top Europe C1 NASA, JSC, Greenbelt, MD USA. Univ London Imperial Coll Sci Technol & Med, London SW7 2AZ, England. Lawrence Livermore Natl Lab, Livermore, CA USA. Univ New Mexico, Albuquerque, NM 87131 USA. Open Univ, Milton Keynes MK7 6AA, Bucks, England. Univ Washington, Seattle, WA 98195 USA. Univ Calif Berkeley, Berkeley, CA 94720 USA. Amer Museum Nat Hist, New York, NY 10024 USA. Case Western Reserve Univ, Cleveland, OH 44106 USA. Univ Chicago, Chicago, IL 60637 USA. Univ Hawaii, Honolulu, HI 96822 USA. Brookhaven Natl Lab, Upton, NY 11973 USA. Univ Sci & Technol Lille, Lille, France. Univ Tokyo, Tokyo, Japan. Kyushu Univ, Fukuoka 812, Japan. Univ Munster, D-4400 Munster, Germany. Naval Res Lab, Washington, DC USA. Kobe Univ, Kobe, Hyogo, Japan. Osaka Univ, Suita, Osaka 565, Japan. US Geol Survey, Washington, DC 20242 USA. Michigan State Univ, E Lansing, MI 48824 USA. EM michael.e.zolensky@nasa.gov RI Dai, Zurong/E-6732-2010; Taheri, Mitra/F-1321-2011; Stroud, Rhonda/C-5503-2008 OI Stroud, Rhonda/0000-0001-5242-8015 NR 0 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 AUG PY 2006 VL 41 IS 8 SU S BP A167 EP A167 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 065PR UT WOS:000239172300314 ER PT J AU Greenhall, CA AF Greenhall, Charles A. TI A Kalman filter clock ensemble algorithm that admits measurement noise SO METROLOGIA LA English DT Article ID TIME SCALE ALGORITHM AB This work gives an algorithm for combining the readings of an ensemble of clocks in which noisy pairwise comparisons are admitted. It extends and generalizes a previously published Kalman filter algorithm that is useful only for an ensemble of clocks within the same laboratory. The present algorithm may be useful for an ensemble of clocks distributed among several remote laboratories. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Greenhall, CA (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr,MS 298-100, Pasadena, CA 91109 USA. EM cgreenhall@jpl.nasa.gov NR 19 TC 13 Z9 13 U1 4 U2 6 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0026-1394 J9 METROLOGIA JI Metrologia PD AUG PY 2006 VL 43 IS 4 SI SI BP S311 EP S321 DI 10.1088/0026-1394/43/4/S19 PG 11 WC Instruments & Instrumentation; Physics, Applied SC Instruments & Instrumentation; Physics GA 072WK UT WOS:000239703500020 ER PT J AU Franklin, RB Mills, AL AF Franklin, Rima B. Mills, Aaron L. TI Structural and functional responses of a sewage microbial community to dilution-induced reductions in diversity SO MICROBIAL ECOLOGY LA English DT Article ID ECOSYSTEM FUNCTION RELATIONSHIP; 16S RIBOSOMAL-RNA; CHLOROFORM FUMIGATION; SPECIES REDUNDANCY; SOIL; BIODIVERSITY; STABILITY; SUSTAINABILITY; POPULATIONS; DISTURBANCE AB The relationship between functional redundancy and microbial community structure-diversity was examined using laboratory incubations to ensure constant environmental conditions. Serial dilutions of a sewage microbial community were prepared, used to inoculate sterile sewage, and maintained in batch culture. Probability suggests that dilution of the initial community should remove rare organism types, creating mixtures of cells differing in diversity. Regrowth of the diluted mixtures generated communities similar in abundance but differing in community structure and relative diversity (as determined using two DNA fingerprinting techniques and dilution-to-extinction analysis of community-level physiological profiles). The in situ function of each regrown community was examined by monitoring the short-term uptake of five different C-14-labeled compounds (glucose, acetate, citrate, palmitic acid, and an amino acid mixture). No significant differences were detected between treatments in either the rate of uptake of a substrate or the efficiency with which each community assimilated each compound. The fact that the activity of the original community was the same as that of a community regrown from an inoculum containing fewer that 100 cells (10(-6) dilution) indicates that functional redundancy was quite high in this system. For each organism type eliminated during the dilution process, at least one of the remaining types was able to provide the same function at the same level as the lost one. Further research is necessary to determine what impact this functional redundancy may have on overall ecosystem function and stability. C1 Univ Virginia, Dept Environm Sci, Charlottesville, VA 22904 USA. NASA, Space Life Sci Lab, Kennedy Space Ctr, FL 32899 USA. RP Mills, AL (reprint author), Univ Virginia, Dept Environm Sci, POB 400123, Charlottesville, VA 22904 USA. EM amills@virginia.edu NR 61 TC 40 Z9 41 U1 2 U2 29 PU SPRINGER PI NEW YORK PA 233 SPRING STREET, NEW YORK, NY 10013 USA SN 0095-3628 J9 MICROB ECOL JI Microb. Ecol. PD AUG PY 2006 VL 52 IS 2 BP 280 EP 288 DI 10.1007/s00248-006-9033-0 PG 9 WC Ecology; Marine & Freshwater Biology; Microbiology SC Environmental Sciences & Ecology; Marine & Freshwater Biology; Microbiology GA 083TL UT WOS:000240481000012 PM 16897310 ER PT J AU Boulet, C Boissoles, J Tipping, RH Ma, Q AF Boulet, C. Boissoles, J. Tipping, R. H. Ma, Q. TI On the temperature dependence of the integrated intensity of the collision-induced fundamental band of O-2-O-2 SO MOLECULAR PHYSICS LA English DT Article; Proceedings Paper CT 19th Colloquium on High Resolution Molecular Spectroscopy CY SEP 11-16, 2005 CL Salamanca, SPAIN ID ABSORPTION-SPECTRA; PAIRS; O-2-N-2; O-2; PARAMETERS; MOLECULES; O-2-CO2; OXYGEN; N-2 AB The temperature dependence of the integrated intensity of the collision-induced fundamental band of O-2-O-2 pairs has been investigated. For T < 280 K, most of the intensity has been shown to arise through the long-range isotropic quadrupolar mechanism, which leads to a monotonic decrease with increasing T. Recent observations carried out at higher temperature show a small increase in the integrated intensity as T increases. Assuming that this increase in absorption is due to a short-range isotropic overlap dipole and fitting the theoretically calculated results to the experimental data, reasonable values are obtained for the magnitude and range of this dipole. The assumption is tested by calculating the corresponding spectral profiles, and it is found that these are in good agreement with the experimental measurements over the temperature range 190K to 350 K. C1 Univ Alabama, Tuscaloosa, AL 35487 USA. Univ Rennes 1, Rennes, France. Univ Paris 11, Orsay, France. Columbia Univ, New York, NY 10027 USA. NASA, Goddard Space Flight Ctr, New York, NY 10025 USA. RP Tipping, RH (reprint author), Univ Alabama, Tuscaloosa, AL 35487 USA. EM rtipping@bama.ua..edu NR 16 TC 1 Z9 1 U1 2 U2 2 PU TAYLOR & FRANCIS LTD PI ABINGDON PA 4 PARK SQUARE, MILTON PARK, ABINGDON OX14 4RN, OXON, ENGLAND SN 0026-8976 J9 MOL PHYS JI Mol. Phys. PD AUG-SEP PY 2006 VL 104 IS 16-17 BP 2753 EP 2758 DI 10.1080/00268970600857792 PG 6 WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical SC Chemistry; Physics GA 078MX UT WOS:000240109000016 ER PT J AU Zhou, D O'Sullivan, D Semones, E Weyland, M AF Zhou, D. O'Sullivan, D. Semones, E. Weyland, M. TI Charge spectra of cosmic ray nuclei measured with CR-39 detectors in Low Earth Orbit SO NUCLEAR INSTRUMENTS & METHODS IN PHYSICS RESEARCH SECTION A-ACCELERATORS SPECTROMETERS DETECTORS AND ASSOCIATED EQUIPMENT LA English DT Article DE cosmic rays; Low Earth Orbit; CR-39 detectors; charge spectra ID AVIATION ALTITUDES AB Galactic Cosmic Rays (GCR) nuclei play an important role in the radiation exposure of humans in Low Earth Orbit (LEO). CR-39 nuclear track detectors have been successfully used to measure the charge spectrum of cosmic rays and related radiation dose in LEO. The method for measuring charge spectrum is based on the analysis of the etch rate gradient and effective etch rate ratio, along with calibration by high-energy heavy ions at particle accelerators. Here we report our results obtained in the interior of spacecraft for the STS-108, STS-112 and ISS-7S missions. Comparisons have been made between experimental and theoretical predictions and show good agreement. (c) 2006 Elsevier B.V. All rights reserved. C1 Johnson Space Ctr, Houston, TX 77058 USA. Univ Space Res Assoc, Houston, TX 77058 USA. Dublin Inst Adv Studies, Dublin 2, Ireland. RP Zhou, D (reprint author), Johnson Space Ctr, Mailcode SF21,2101 Nasa Rd 1, Houston, TX 77058 USA. EM dzhou@ems.jsc.nasa.gov NR 12 TC 12 Z9 13 U1 0 U2 0 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 AUG 1 PY 2006 VL 564 IS 1 BP 262 EP 266 DI 10.1016/j.nima.2006.05.044 PG 5 WC Instruments & Instrumentation; Nuclear Science & Technology; Physics, Nuclear; Physics, Particles & Fields SC Instruments & Instrumentation; Nuclear Science & Technology; Physics GA 072JK UT WOS:000239669500032 ER PT J AU Emfietzoglou, D Nikjoo, H Pathak, A AF Emfietzoglou, D. Nikjoo, H. Pathak, A. TI Electronic cross sections for proton transport in liquid water based on optical-data models SO NUCLEAR INSTRUMENTS & METHODS IN PHYSICS RESEARCH SECTION B-BEAM INTERACTIONS WITH MATERIALS AND ATOMS LA English DT Article; Proceedings Paper CT 17th International Conference on Ion Beam Analysis CY JUN 26-JUL 01, 2005 CL Seville, SPAIN SP Univ Autonoma Madrid, Univ Sevilla, Junta Andalucia, Minist Educ & Ciencia, Consejo Superior Investigaciones Cient, Int Atomic Energy Agcy, European Act COST G8, Boem Phys Soc, High Voltage Engn Europa BV, Banco Santander Cent Hispano, Schering Espana DE protons; water; dielectric; optical data ID ENERGETIC PROTONS; CONDENSED MATTER; STOPPING POWER; SCATTERING AB We compare differential, integrated and stopping electronic cross sections for (non-relativistic) proton impact in liquid water calculated by two different optical-data models using reflectance and Compton scattering data. The complex dielectric response function over the energy-momentum plane is obtained by a sum-rule constrained extended-Drude scheme, which fits the optical data and preserves the Bethe ridge. Higher order Z-corrections were implemented for extending the stopping calculations down to the Bragg peak. The construction of molecular cross sections allows the contribution of each electronic channel to the stopping process to be calculated and the need to separately evaluate the shell corrections is overcome. The present study complements our previous work on the influence of dispersion to proton inelastic characteristics and provides further insight on the application of the dielectric methodology to proton electronic losses in condensed biological materials. (c) 2006 Elsevier B.V. All rights reserved. C1 Univ Ioannina, Sch Med, Dept Med Phys, GR-45110 Ioannina, Greece. NASA, Lyndon B Johnson Space Ctr, Ctr Adv Space Studies, USRA, Houston, TX 77058 USA. Univ Hyderabad, Sch Phys, Hyderabad 500046, Andhra Pradesh, India. RP Emfietzoglou, D (reprint author), Univ Ioannina, Sch Med, Dept Med Phys, GR-45110 Ioannina, Greece. EM demfietz@cc.uoi.gr RI Emfietzoglou, Dimitris/G-7168-2012 NR 13 TC 13 Z9 13 U1 0 U2 0 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0168-583X J9 NUCL INSTRUM METH B JI Nucl. Instrum. Methods Phys. Res. Sect. B-Beam Interact. Mater. Atoms PD AUG PY 2006 VL 249 BP 26 EP 28 DI 10.1016/j.nimb.2006.03.015 PG 3 WC Instruments & Instrumentation; Nuclear Science & Technology; Physics, Atomic, Molecular & Chemical; Physics, Nuclear SC Instruments & Instrumentation; Nuclear Science & Technology; Physics GA 070ST UT WOS:000239545000007 ER PT J AU Berger, P Gallien, JP Khodja, H Daudin, L Berger, MH Sayir, A AF Berger, P. Gallien, J-P. Khodja, H. Daudin, L. Berger, M-H. Sayir, A. TI Hydrogen incorporation into high temperature protonic conductors: Nuclear microprobe microanalysis by means of (1)H(p,p)(1)H scattering SO NUCLEAR INSTRUMENTS & METHODS IN PHYSICS RESEARCH SECTION B-BEAM INTERACTIONS WITH MATERIALS AND ATOMS LA English DT Article; Proceedings Paper CT 17th International Conference on Ion Beam Analysis CY JUN 26-JUL 01, 2005 CL Seville, SPAIN SP Univ Autonoma Madrid, Univ Sevilla, Junta Andalucia, Minist Educ & Ciencia, Consejo Super Invest Cient, Int Atom Energy Agcy, European Act COST G8, Boem Phys Soc, High Voltage Engn Europa BV, Banco Santander Cent Hispano, Schering Espana DE hydrogen; forward scattering; perovskite; microprobe ID RECOIL COINCIDENCE SPECTROMETRY; MICROSCOPY AB Protonic conductivity of some solid state materials at an intermediate temperature range (400-600 degrees C), referred as high temperature protonic conductor (HTPC), suggests their application as electrolytes in electrochemical cells, batteries, sensors, etc. Among them, some perovskites can be protonic and electronic conductors. Several obstacles remain to achieve the full potential of these ceramic membranes, among them the lack of measurement techniques and of an unambiguous model for conductivity. A precise understanding of the transport mechanisms requires local profiling of hydrogen concentrations within the microstructure of the ceramic. We have used the nuclear microprobe of the Laboratoire Pierre SCE to investigate quantitatively the spatial distribution of hydrogen after water heat treatment of textured perovskites, SrCe(0.9)Y(0.1)O(3-delta) and Sr(3)Ca(1+x)Nb(2-x)O(9-delta), x = 0.18, synthesized according to a meltprocess developed at NASA GRC. A not very common method has been developed for hydrogen measurements in thin samples, (1)H(p,p)(1)H elastic recoil coincidence spectrometry (ERCS). Early experiments have evidenced hydrogen concentration enhancement within grain boundaries. (c) 2006 Elsevier B.V. All rights reserved. C1 CEA Saclay, CNRS, Lab Pierre SUE, F-91191 Gif Sur Yvette, France. Ecole Mines Paris, Ctr PM Fourt, F-91003 Evry, France. NASA, GRC, CWRU, Cleveland, OH 44135 USA. RP Berger, P (reprint author), CEA Saclay, CNRS, Lab Pierre SUE, F-91191 Gif Sur Yvette, France. EM pascal.berger@cea.fr RI DAUDIN, laurent/A-8801-2008; Berger, Marie-Helene/B-9785-2013; Khodja, Hicham/A-1869-2016 NR 17 TC 3 Z9 3 U1 2 U2 4 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0168-583X J9 NUCL INSTRUM METH B JI Nucl. Instrum. Methods Phys. Res. Sect. B-Beam Interact. Mater. Atoms PD AUG PY 2006 VL 249 BP 527 EP 531 DI 10.1016/j.nimb.2006.03.045 PG 5 WC Instruments & Instrumentation; Nuclear Science & Technology; Physics, Atomic, Molecular & Chemical; Physics, Nuclear SC Instruments & Instrumentation; Nuclear Science & Technology; Physics GA 070ST UT WOS:000239545000131 ER PT J AU Emfietzoglou, D Nikjoo, H Papamichael, G Pathak, A AF Emfietzoglou, D. Nikjoo, H. Papamichael, G. Pathak, A. TI Proton beam profiling in soft biological matter by detailed Monte Carlo simulation SO NUCLEAR INSTRUMENTS & METHODS IN PHYSICS RESEARCH SECTION B-BEAM INTERACTIONS WITH MATERIALS AND ATOMS LA English DT Article; Proceedings Paper CT 17th International Conference on Ion Beam Analysis CY JUN 26-JUL 01, 2005 CL Seville, SPAIN SP Univ Autonoma Madrid, Univ Sevilla, Junta Andalucia, Minist Educ & Ciencia, Consejo Superior Investigaciones Cient, Int Atomic Energy Agcy, European Act COST G8, Boem Phys Soc, High Voltage Engn Europa BV, Banco Santander Cent Hispano, Schering Espana DE Monte Carlo; microdosimetry; protons; water ID HEAVY-IONS; WATER AB Distributions of relevance to proton beam profiling in soft biological matter are obtained by our Monte Carlo track structure code (MC4), which simulates in an event-by-event mode the electronic losses of light ions and all their secondary electrons in water. We present results on electronic energy density and clustering of interaction events around MeV proton tracks which are associated with important "local track" parameters. The detailed character of the simulation based on single-collision cross sections for all the elementary interaction processes allows a probing resolution of the order of nanometers. Since soft biological tissue exists in a liquid/solid like state we compare results obtained by both the oscillator strength properties of the water molecule and the dielectric response of liquid water. Their differences in terms of the nanometric pattern of proton tracks is examined. (c) 2006 Elsevier B.V. All rights reserved. C1 Univ Ioannina, Sch Med, Dept Med Phys, GR-45110 Ioannina, Greece. NASA, Lyndon B Johnson Space Ctr, USRA, Ctr Adv Space Studies, Houston, TX 77058 USA. Natl Tech Univ Athens, Dept Mech Engn, GR-15710 Athens, Greece. Univ Hyderabad, Sch Phys, Hyderabad 500046, Andhra Pradesh, India. RP Emfietzoglou, D (reprint author), Univ Ioannina, Sch Med, Dept Med Phys, GR-45110 Ioannina, Greece. EM demfietz@cc.uoi.gr RI Emfietzoglou, Dimitris/G-7168-2012 NR 7 TC 4 Z9 4 U1 0 U2 1 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0168-583X J9 NUCL INSTRUM METH B JI Nucl. Instrum. Methods Phys. Res. Sect. B-Beam Interact. Mater. Atoms PD AUG PY 2006 VL 249 BP 670 EP 672 DI 10.1016/j.nimb.2006.03.055 PG 3 WC Instruments & Instrumentation; Nuclear Science & Technology; Physics, Atomic, Molecular & Chemical; Physics, Nuclear SC Instruments & Instrumentation; Nuclear Science & Technology; Physics GA 070ST UT WOS:000239545000162 ER PT J AU Feng, H Vandemark, D Quilfen, Y Chapron, B Beckley, B AF Feng, Hui Vandemark, Doug Quilfen, Yves Chapron, Bertrand Beckley, Brian TI Assessment of wind-forcing impact on a global wind-wave model using the TOPEX altimeter SO OCEAN ENGINEERING LA English DT Article DE wave modeling; altimeter; scatterometer; wind forcing; sea state bias ID SEA-STATE BIAS; SCATTEROMETER WINDS; SATELLITE DATA; IN-SITU; IMPLEMENTATION; ASSIMILATION; VARIABILITY; SENSITIVITY; SPECTRA; LEVEL AB The study presents assessment of an operational wave model (Wavewatch III), focusing upon the model sensitivity to wind-forcing products. Four wind fields are used to drive the model, including the NCEP/NCAR reanalysis and three other products that assimilate various satellite wind measurements having high spatial resolution, including the QuikSCAT scatterometer. Three wave field statistics: significant wave height, mean zero-crossing wave period, and mean square slope are compared with collocated TOPEX altimeter derivatives to gauge the relative skill of differing wind-forced model runs, as well as to demonstrate an extended use of the altimeter beyond simply supplying wave height for wave model validation and assimilation. Results suggest that model output is critically sensitive to choice of the wind field product. Higher spatial resolution in the wind fields does lead to improved agreement for the higher-order wave statistics. (C) 2005 Elsevier Ltd. All rights reserved. C1 Hampton Univ, Ctr Atmospher Sci, Hampton, VA 23668 USA. NASA, Goddard Space Flight Ctr, Wallops Isl, VA 23337 USA. IFREMER, Ctr Brest, Plouzane, France. RP Feng, H (reprint author), Hampton Univ, Ctr Atmospher Sci, Hampton, VA 23668 USA. EM hui.feng@unh.Edu RI Chapron, Bertrand/O-6527-2015; Quilfen, Yves/A-1824-2016 NR 39 TC 18 Z9 20 U1 0 U2 3 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0029-8018 J9 OCEAN ENG JI Ocean Eng. PD AUG PY 2006 VL 33 IS 11-12 BP 1431 EP 1461 DI 10.1016/j.oceaneng.2005.10.015 PG 31 WC Engineering, Marine; Engineering, Civil; Engineering, Ocean; Oceanography SC Engineering; Oceanography GA 069KJ UT WOS:000239444600002 ER PT J AU Tian, JL Cook, WB AF Tian, Jialin Cook, William B. TI Recovery of overlapped spectral harmonics in multiplex Fabry-Perot interferometry SO OPTICAL ENGINEERING LA English DT Article DE multiplex Fabry-Perot interferometer; multiresolution analysis; overlapping multiplex Fabry-Perot interferometer spectral harmonics; spectrum recovery algorithm AB We propose an algorithm for recovering the overlapped harmonic components of a multiplex Fabry-Perot interferometer (MFPI) spectrum. A potential solution that utilizes the multiresolution properties of the MFPI spectrum is presented. The corrupted harmonic components are detected by comparing consecutive harmonic pairs at the same sampling rate and window length. The overlapped spectral components are adjusted with correction terms that have been determined from the detection stage. (c) 2006 Society of Photo-Optical Instrumentation Engineers. C1 NASA, Langley Res Ctr, Sci Applicat Int Corp, Hampton, VA 23681 USA. RP Tian, JL (reprint author), NASA, Langley Res Ctr, Sci Applicat Int Corp, Mail Stop 468,5 N Dryden St, Hampton, VA 23681 USA. EM j.tian@larc.nasa.gov NR 5 TC 0 Z9 0 U1 0 U2 3 PU SPIE-INT SOCIETY OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98225 USA SN 0091-3286 J9 OPT ENG JI Opt. Eng. PD AUG PY 2006 VL 45 IS 8 AR 085601 DI 10.1117/1.2338594 PG 6 WC Optics SC Optics GA 093IN UT WOS:000241162100037 ER PT J AU Smith, DD Lepeshkin, NN Schweinsberg, A Gehring, G Boyd, RW Park, QH Chang, H Jackson, DJ AF Smith, David D. Lepeshkin, N. N. Schweinsberg, A. Gehring, G. Boyd, R. W. Park, Q-Han Chang, Hongrok Jackson, D. J. TI Coupled-resonator-induced transparency in a fiber system SO OPTICS COMMUNICATIONS LA English DT Article ID ELECTROMAGNETICALLY INDUCED TRANSPARENCY; EXCEPTIONAL POINTS; RING LASER AB Mode splitting in two coupled fiber-ring resonators is observed. We observe a cancellation of on-resonance absorption, which can be interpreted as resulting from the destructive interference of the symmetric and anti-symmetric modes of the system, in analogy with electromagnetically-induced transparency in atoms. The response of the system is characterized according to the degeneracy and distinguishability of the normal modes. Finite-difference time-domain simulations agree with an analysis of the transient response of the intra-cavity fields, and reveal coherent oscillations of the photons between the resonators, i.e., under-damped Rabi oscillations, which we predict to occur for distinguishable mode splittings. (c) 2006 Elsevier B.V. All rights reserved. C1 Univ New Mexico, Dept Phys & Astron, Albuquerque, NM 87131 USA. Univ Rochester, Inst Opt, Rochester, NY 14627 USA. Korea Univ, Dept Phys, Seoul 136701, South Korea. Univ Alabama, Dept Phys, Huntsville, AL 35899 USA. NASA, George C Marshall Space Flight Ctr, Sci Directorate, Huntsville, AL 35812 USA. Jet Prop Lab, Quantum Comp Technol Grp, Pasadena, CA 91109 USA. RP Smith, DD (reprint author), Univ New Mexico, Dept Phys & Astron, Albuquerque, NM 87131 USA. EM david.d.smith@nasa.gov RI liu, ze/A-2322-2010; Schweinsberg, Aaron/D-7488-2012 NR 27 TC 18 Z9 22 U1 3 U2 10 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0030-4018 J9 OPT COMMUN JI Opt. Commun. PD AUG 1 PY 2006 VL 264 IS 1 BP 163 EP 168 DI 10.1016/j.optcom.2006.02.037 PG 6 WC Optics SC Optics GA 069VQ UT WOS:000239477300024 ER PT J AU Jelenkovic, BM Chung, S Prestage, JD Maleki, L AF Jelenkovic, B. M. Chung, S. Prestage, J. D. Maleki, L. TI High-resolution microwave-optical double-resonance spectroscopy of hyperfine splitting of trapped (113)Cd(+) ions SO PHYSICAL REVIEW A LA English DT Article ID CLOCKS AB We performed double resonance spectroscopy on the ground-state hyperfine splitting of (113)Cd(+) ions trapped in a rf linear trap. The ions were optically pumped by UV light from the (106)Cd lamp and cooled by He buffer gas. The ground-state hyperfine splitting was measured to be 15 199 862 855 Hz with the precision of 1.3x10(-11). The uncertainty stems from the error in extrapolation to zero magnetic field and from the resonance linewidth. This value is 3 Hz lower than the previous high-precision measurements by [Tanaka , Phys. Rev. A 53, 3982 (1996)], in which the laser light was used for optical excitation. The potential for a new microwave frequency standard based on the 15.2-GHz ground-state hyperfine splitting of (113)Cd(+) ions is also discussed. Stability of the hyperfine frequency of (113)Cd(+) ion, with microwaves locked to the hydrogen maser, is similar to 2x10(-13)tau(-1/2). C1 Jet Prop Lab, San Marino, CA 91108 USA. Inst Phys, Belgrade 11001, Serbia. RP Jelenkovic, BM (reprint author), Jet Prop Lab, 4800 Oak Grove Dr, San Marino, CA 91108 USA. NR 14 TC 17 Z9 17 U1 1 U2 6 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 AUG PY 2006 VL 74 IS 2 AR 022505 DI 10.1103/PhysRevA.74.022505 PG 5 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA 080HK UT WOS:000240238300054 ER PT J AU Robbins, DL Beiersdorfer, P Faenov, AY Pikuz, TA Thorn, DB Chen, H Reed, KJ Smith, AJ Boyce, KR Brown, GV Kelley, RL Kilbourne, CA Porter, FS AF Robbins, D. L. Beiersdorfer, P. Faenov, A. Ya. Pikuz, T. A. Thorn, D. B. Chen, H. Reed, K. J. Smith, A. J. Boyce, K. R. Brown, G. V. Kelley, R. L. Kilbourne, C. A. Porter, F. S. TI Polarization measurements of the Lyman-alpha(1) x-ray emission lines of hydrogenlike Ar17+ and Fe25+ at high electron-impact energies SO PHYSICAL REVIEW A LA English DT Article ID BEAM ION-TRAP; CHARGED IONS; HE-LIKE; SPECTROMETER; PLASMA; SPECTROPOLARIMETRY; SPECTROSCOPY; TRANSITIONS; EXCITATION; SUBLEVELS AB We have measured the polarization of the 2p(3/2)-> 1s(1/2) Lyman-alpha(1) x-ray line of hydrogenlike Ar17+ and Fe25+ at electron-impact energies ranging from 7 to 25 threshold units. The highly charged argon and iron ions were produced using the Lawrence Livermore National Laboratory SuperEBIT electron beam ion trap. A combination of two crystal spectrometers and a microcalorimeter were used to record the Lyman-alpha x-ray emission of Ar17+ and Fe25+ and to infer the polarization of the Lyman-alpha(1) line. Our results show a systematic discrepancy with the predictions of distorted-wave calculations. C1 Morehouse Coll, Dept Phys, Atlanta, GA 30314 USA. Lawrence Livermore Natl Lab, Livermore, CA 94550 USA. VNIIFTRI, Multicharged Ions Spectra Data Ctr, Mendeleyevsk 141570, Moscow Region, Russia. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Robbins, DL (reprint author), Morehouse Coll, Dept Phys, Atlanta, GA 30314 USA. RI Porter, Frederick/D-3501-2012; Kelley, Richard/K-4474-2012 OI Porter, Frederick/0000-0002-6374-1119; NR 27 TC 41 Z9 41 U1 1 U2 3 PU AMERICAN 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 AUG PY 2006 VL 74 IS 2 AR 022713 DI 10.1103/PhysRevA.74.022713 PG 5 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA 080HK UT WOS:000240238300074 ER PT J AU Bachlechner, ME Srivastava, D Owens, ET Schiffbauer, J Anderson, JT Burky, MR Ducatman, SC Gripper, AM Guffey, EJ Ramos, FS AF Bachlechner, Martina E. Srivastava, Deepak Owens, Eli T. Schiffbauer, Jarrod Anderson, Jonas T. Burky, Melissa R. Ducatman, Samuel C. Gripper, Adam M. Guffey, Eric J. Ramos, Fernando Serrano TI Mechanisms of pit formation at strained crystalline Si(111)/Si3N4(0001) interfaces: Molecular-dynamics simulations SO PHYSICAL REVIEW B LA English DT Article ID SILICON-NITRIDE; ELECTRONIC-STRUCTURE; BRITTLE-FRACTURE; CHARGE-TRANSFER; THIN-FILMS; SURFACE; GROWTH; DEFECTS; FLUORINATION; DEFORMATION AB Molecular-dynamics simulations of the crystalline silicon-silicon nitride interfaces are performed to investigate the mechanical failure mechanisms at the interfaces under external strain. At 8% applied tensile strain, parallel to the interface, regular crack initiation and propagation in silicon nitride and dislocation emission and propagation in silicon are observed. At larger 16% strain, however, the formation of a pit similar to that in experiments with lattice-mismatched systems is observed. The simulation results suggest the primary mechanism of pit formation is interaction of a local compressional pinch of the film at the interface with the close proximity to the arrival of a dislocation at the interface in the highly strained silicon. C1 W Virginia Univ, Phys Dept, Morgantown, WV 26506 USA. NASA Ames Res Ctr, Moffett Field, CA 94035 USA. Davis & Elkins Coll, Chem Dept, Elkins, WV 26241 USA. Univ High Sch, Morgantown, WV 26505 USA. Metropolitan Univ, Dept Comp Sci, San Juan, PR 00928 USA. RP Bachlechner, ME (reprint author), W Virginia Univ, Phys Dept, Morgantown, WV 26506 USA. NR 63 TC 7 Z9 7 U1 1 U2 5 PU AMERICAN 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 AUG PY 2006 VL 74 IS 7 AR 075327 DI 10.1103/PhysRevB.74.075327 PG 6 WC Physics, Condensed Matter SC Physics GA 080HP UT WOS:000240238800078 ER PT J AU Yeh, NC Strayer, DM AF Yeh, N. -C. Strayer, D. M. TI Reply to "Comment on 'Microwave vortex dissipation of superconducting Nd-Ce-Cu-O epitaxial films in high magnetic fields' " SO PHYSICAL REVIEW B LA English DT Editorial Material ID YBA2CU3O7 SINGLE-CRYSTALS; HIGH-TEMPERATURE SUPERCONDUCTORS; DOPED CUPRATE SUPERCONDUCTORS; AMORPHOUS MO3SI FILMS; BOSE-GLASS TRANSITION; SURFACE IMPEDANCE; II SUPERCONDUCTORS; CRITICAL-DYNAMICS; COLUMNAR DEFECTS; FLUX CREEP AB We demonstrate with detailed analysis that the criticisms in the preceding Comment by Blackstead are largely due to insufficient understanding of the experimental issues associated with our system or the imposition of formalism that is inapplicable to our experiments. In particular, we distinguish the conventional formalism for "field-defined" surface resistance applicable to measurements on samples with filling factors (i.e., the ratio of the sample volume to that of the microwave cavity) approaching 1 from our "dissipation-defined" surface resistance derived from first principles for measurements on samples with very small filling factors. C1 CALTECH, Dept Phys, Pasadena, CA 91125 USA. CALTECH, Jet Prop Lab, Pasadena, CA 91107 USA. RP Yeh, NC (reprint author), CALTECH, Dept Phys, Pasadena, CA 91125 USA. NR 27 TC 0 Z9 0 U1 0 U2 3 PU AMERICAN 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 AUG PY 2006 VL 74 IS 6 AR 066502 DI 10.1103/PhysRevB.74.066502 PG 8 WC Physics, Condensed Matter SC Physics GA 080HM UT WOS:000240238500084 ER PT J AU Akylas, E Kassinos, SC Langer, CA AF Akylas, E. Kassinos, S. C. Langer, C. A. TI An analytical solution for rapidly distorted turbulent shear flow in a rotating frame SO PHYSICS OF FLUIDS LA English DT Article ID LINEAR-THEORY; FIELD AB In this study we apply rapid distortion theory to the case of nonstratified homogeneous turbulence that is sheared in a frame that counter-rotates at a rate that matches in magnitude the rotation associated with the mean shear. In the inviscid case, analytical solutions are worked out for the evolution of the components of the Reynolds stresses and the structure dimensionality tensor, and these are shown to equal each other. The results are compared to direct numerical simulations data with which they proved to be in good agreement, especially in terms of the Reynolds shear stress and of the dimensionless tensor components. Finally, the development of the structure of a passive scalar field with a constant mean gradient is investigated, and remarkable analogies are shown to exist between this case and the case of shear in a fixed frame. (c) 2006 American Institute of Physics. C1 Univ Cyprus, Dept Mech & Mfg Engn, CY-1678 Nicosia, Cyprus. Natl Observ Athens, Inst Environm Res, Athens, Greece. Stanford Univ, NASA, Ctr Turbulence Res, Stanford, CA 94305 USA. RP Akylas, E (reprint author), Univ Cyprus, Dept Mech & Mfg Engn, 75 Kallipoleos, CY-1678 Nicosia, Cyprus. RI Kassinos, Stavros/B-6404-2016; Akylas, Evangelos/E-4418-2016 OI Kassinos, Stavros/0000-0002-3501-3851; Akylas, Evangelos/0000-0002-2731-657X NR 19 TC 4 Z9 4 U1 1 U2 2 PU AMER INST PHYSICS PI MELVILLE PA CIRCULATION & FULFILLMENT DIV, 2 HUNTINGTON QUADRANGLE, STE 1 N O 1, MELVILLE, NY 11747-4501 USA SN 1070-6631 EI 1089-7666 J9 PHYS FLUIDS JI Phys. Fluids PD AUG PY 2006 VL 18 IS 8 AR 085104 DI 10.1063/1.2265010 PG 11 WC Mechanics; Physics, Fluids & Plasmas SC Mechanics; Physics GA 080HB UT WOS:000240237400030 ER PT J AU Cambon, C Rubinstein, R AF Cambon, Claude Rubinstein, Robert TI Anisotropic developments for homogeneous shear flows SO PHYSICS OF FLUIDS LA English DT Article ID NON-ISOTROPIC TURBULENCE; AXISYMMETRIC TURBULENCE; RAPID DISTORTION; SPECTRUM; MODEL AB The general decomposition of the spectral correlation tensor R-ij(k) by Cambon [J. Fluid Mech. 202, 295 (1989); 337, 303 (1997)] into directional and polarization components is applied to the representation of R-ij(k) by spherically averaged quantities. The decomposition splits the deviatoric part H-ij(k) of the spherical average of R-ij(k) into directional and polarization components H-ij((e))(k) and H-ij((z))(k). A self-consistent representation of the spectral tensor is constructed in terms of these spherically averaged quantities. The directional and polarization components must be treated independently: representation of the spectral tensor using the spherical average H-ij(k) alone proves to be inconsistent with Navier-Stokes dynamics. In particular, a spectral tensor consistent with a prescribed Reynolds stress is not unique. Since spherical averaging entails a loss of information, the description of an anisotropic correlation tensor by spherical averages is limited to weak departures from isotropy. The degree of anisotropy permitted is restricted by realizability requirements. More general descriptions can be given using a higher-order expansion of the spectral tensor. Directionality is described by a conventional expansion in spherical harmonics, but polarization requires an expansion in special tensorial quantities generated by irreducible representations of the rotation group SO3. These expansions are considered in more detail in the special case of axial symmetry. (c) 2006 American Institute of Physics. C1 Ecole Cent Lyon, UMR 5509, LMFA, F-69134 Ecully, France. NASA, Langley Res Ctr, Computat Aerosci Branch, Hampton, VA 23681 USA. RP Cambon, C (reprint author), Ecole Cent Lyon, UMR 5509, LMFA, F-69134 Ecully, France. NR 29 TC 24 Z9 24 U1 0 U2 6 PU AMER INST PHYSICS PI MELVILLE PA CIRCULATION & FULFILLMENT DIV, 2 HUNTINGTON QUADRANGLE, STE 1 N O 1, MELVILLE, NY 11747-4501 USA SN 1070-6631 J9 PHYS FLUIDS JI Phys. Fluids PD AUG PY 2006 VL 18 IS 8 AR 085106 DI 10.1063/1.2265012 PG 11 WC Mechanics; Physics, Fluids & Plasmas SC Mechanics; Physics GA 080HB UT WOS:000240237400032 ER PT J AU Zhang, J Wu, XL Rashidnia, N AF Zhang, Jie Wu, X. L. Rashidnia, Nasser TI Thermal radiation and thickness fluctuations in freely suspended liquid films SO PHYSICS OF FLUIDS LA English DT Article ID RAYLEIGH-BENARD CONVECTION; FLOWING SOAP FILM; TURBULENT CONVECTION; PASSIVE SCALAR; 2-DIMENSIONAL TURBULENCE; DYNAMICS; VELOCITY; SPECTRA; TEMPERATURE; HYPOTHESES AB Thermal convection in a vertically suspended soap film subjected to a vertical temperature gradient is marked by intense density fluctuations delta rho(2), uncommon to laboratory Rayleigh-Benard convection (RBC). Such large fluctuations result from stratification in the film under the influence of gravity. Herein we present the first direct measurement of two-dimensional density fluctuations in a free-standing soap film using a single-point infrared detector. The radiation densitometer is nonintrusive and responds instantaneously to local density variations. Measurements of the power spectrum Gamma(f) of delta rho(2) are carried out using a variety of sample geometries of the aspect ratio of unity. In all cases, Gamma(f) scales with the frequency as f(-1.4 +/- 0.1) in the low frequency regime, which is in good agreement with the Bolgiano's theoretical prediction for a stably stratified fluid. Combining thermal imaging and particle tracking, we also show that it is feasible to measure the full-field density flux j(x,y)=rho(2)(x,y)v(x,y) in the film. Despite that individual snapshots of j(x,y) appear random, the time-averaged flux forms a close loop similar to the large-scale circulation commonly seen in RBC, when a sufficiently large temperature gradient is present. (c) 2006 American Institute of Physics. C1 Univ Pittsburgh, Dept Phys, Pittsburgh, PA 15260 USA. NASA, Glenn Res Ctr, Natl Ctr Micrograv Res, Cleveland, OH 44135 USA. RP Zhang, J (reprint author), Univ Pittsburgh, Dept Phys, Pittsburgh, PA 15260 USA. RI Zhang, Jie/O-2127-2015 NR 54 TC 11 Z9 11 U1 2 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 1070-6631 J9 PHYS FLUIDS JI Phys. Fluids PD AUG PY 2006 VL 18 IS 8 AR 085110 DI 10.1063/1.2337997 PG 13 WC Mechanics; Physics, Fluids & Plasmas SC Mechanics; Physics GA 080HB UT WOS:000240237400036 ER PT J AU Park, SY Seywald, H Krizan, SA Stillwagen, FH AF Park, Sang-Young Seywald, Hans Krizan, Shawn A. Stillwagen, Frederic H. TI Mission design for human outer planet exploration (HOPE) using a magnetoplasma spacecraft SO PLANETARY AND SPACE SCIENCE LA English DT Article DE mission design; interplanetary trajectory; Human Outer Planet Exploration; trajectory optimization ID LOW-THRUST; OPTIMIZATION; TRAJECTORIES; CONSTRAINTS; PROPULSION; TRANSFERS AB To send humans beyond Mars, a Human Outer Planet Exploration (HOPE) mission has been studied for new spacecraft concepts and technologies. In this paper, an interplanetary trajectory and a preliminary spacecraft design are presented for the HOPE visit to Callisto, one of Jupiter's moons. To design a round-trip trajectory for the mission, the characteristics of the spacecraft and its trajectories are analyzed. A detailed optimization approach is formulated to utilize a Variable Specific Impulse Magnetoplasma Rocket (VASIMR) engine with capabilities of variable specific impulse, variable engine efficiency, and engine on-off control. It is mainly illustrated that a 30 MW powered spacecraft can make the mission possible in a 5-year round trip constraint around the year 2045. Trajectories with different power and reactor options are also discussed. The results obtained in this study can be used for formulating an overall concept for the mission. (c) 2006 Published by Elsevier Ltd. C1 Yonsei Univ, Dept Astron & Space Sci, Seoul 120749, South Korea. Analyt Mech Associates Inc, Hampton, VA 23666 USA. NASA, Langley Res Ctr, Hampton, VA 23681 USA. RP Park, SY (reprint author), Yonsei Univ, Dept Astron & Space Sci, Seoul 120749, South Korea. EM spark@galaxy.yonsei.ac.kr NR 24 TC 4 Z9 4 U1 1 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 AUG PY 2006 VL 54 IS 8 BP 737 EP 749 DI 10.1016/j.pss.2006.04.006 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 075EV UT WOS:000239867400003 ER PT J AU Kruger, H Bindschadler, D Dermott, SF Graps, AL Grun, E Gustafson, BA Hamilton, DP Hanner, MS Horanyi, M Kissel, J Lindblad, BA Linkert, D Linkert, G Mann, I McDonnell, JAM Moissl, R Morfill, GE Polanskey, C Schwehm, G Srama, R Zook, HA AF Krueger, H. Bindschadler, D. Dermott, S. F. Graps, A. L. Gruen, E. Gustafson, B. A. Hamilton, D. P. Hanner, M. S. Horanyi, M. Kissel, J. Lindblad, B. A. Linkert, D. Linkert, G. Mann, I. McDonnell, J. A. M. Moissl, R. Morfill, G. E. Polanskey, C. Schwehm, G. Srama, R. Zook, H. A. TI Galileo dust data from the jovian system: 1997-1999 SO PLANETARY AND SPACE SCIENCE LA English DT Article DE interplanetary dust; circumplanetary dust; dust streams; Jupiter dust; dust clouds ID PLANETARY SATELLITES; INTERSTELLAR DUST; ULYSSES; STREAMS; MAGNETOSPHERE; DETECTOR; CLOUDS; INTERPLANETARY; JUPITER; GRAINS AB The dust detector system on board the Galileo spacecraft recorded dust impacts in circumjovian space during the craft's orbital mission about Jupiter. This is the eighth in a series of papers dedicated to presenting Galileo and Ulysses dust data. We present data from the Galileo dust instrument for the period January 1997-December 1999 when the spacecraft completed 21 revolutions about Jupiter. In this time interval data were obtained as high resolution realtime science data or recorded data during 449 days (representing 41% of the entire period), or via memory readouts during the remaining times. Because the data transmission rate of the spacecraft was very low, the complete data set (i.e. all parameters measured by the instrument during impact of a dust particle) of only 3% (7625) of all particles detected could be transmitted to Earth; the other particles were only counted. Together with the data of 2883 particles detected during, Galileo's interplanetary cruise and 53 53 particles detected in the jovian system in 1996, complete data of 15 861 particles detected by the Galileo dust instrument from 1989 to 1999 are now available. The majority of the detected particles were tiny grains (about 10 nm in radius), most of them originating from Jupiter's innermost Galilean moon Io. They were detected throughout the jovian system and the highest impact rates exceeded 100 min(-1) (C21 orbit; 01 July 1999). With the new data set the times of onset, cessation and a 180 degrees shift in the impact direction of the grains measured during 19 Galileo orbits about Jupiter are well reproduced by simulated 9 nm particles charged up to a potential of +3 V, confirming earlier results obtained for only two Galileo orbits (Horanyi, M., Grun, E., Heck, A., 1997. Modeling the Galileo dust measurements at Jupiter. Geophys. Res. Lett. 24, 2175-2178). Galileo has detected a large number of bigger particles mostly in the region between the Galilean moons. The average radius of 370 of these grains measured in the 1996-1999 period is about 2 mu m (assuming spherical grains with density 1 g cm(-3)) and the size distribution rises steeply towards smaller grains. The biggest detected particles have a radius of about 10 mu m. (c) 2006 Elsevier Ltd. All rights reserved. C1 Max Planck Inst Sonnensystemforsch, D-37191 Katlenburg Lindau, Germany. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. Univ Florida, Gainesville, FL 32609 USA. Ist Fis Spazio Interplanetario, INAF, ARTOV, I-00133 Rome, Italy. Max Planck Inst Kernphys, D-69029 Heidelberg, Germany. Hawaii Inst Geophys & Planetol, Honolulu, HI 96822 USA. Univ Maryland, College Pk, MD 20742 USA. Univ Colorado, Atmospher & Space Phys Lab, Boulder, CO 80309 USA. Lund Observ, S-221 Lund, Sweden. Univ Munster, Inst Planetol, D-48149 Munster, Germany. Open Univ, Planetary & Space Sci Res Inst, Milton Keynes MK7 6AA, Bucks, England. Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. Estec, NL-2200 AG Noordwijk, Netherlands. NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. RP Kruger, H (reprint author), Max Planck Inst Sonnensystemforsch, D-37191 Katlenburg Lindau, Germany. EM krueger@mps.mpg.de RI Gustafson, Bo/B-9526-2011; OI Horanyi, Mihaly/0000-0002-5920-9226 NR 49 TC 8 Z9 8 U1 0 U2 1 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 AUG PY 2006 VL 54 IS 9-10 BP 879 EP 910 DI 10.1016/j.pss.2006.04.010 PG 32 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 088BJ UT WOS:000240786200005 ER PT J AU Kruger, H Altobelli, N Anweiler, B Dermott, SF Dikarev, V Graps, AL Grun, E Gustafson, BA Hamilton, DP Hanner, MS Horanyi, M Kissel, J Landgraf, M Lindblad, BA Linkert, D Linkert, G Mann, I McDonnell, JAM Morfill, GE Polanskey, C Schwehm, G Srama, R Zook, HA AF Krueger, H. Altobelli, N. Anweiler, B. Dermott, S. F. Dikarev, V. Graps, A. L. Gruen, E. Gustafson, B. A. Hamilton, D. P. Hanner, M. S. Horanyi, M. Kissel, J. Landgraf, M. Lindblad, B. A. Linkert, D. Linkert, G. Mann, I. McDonnell, J. A. M. Morfill, G. E. Polanskey, C. Schwehm, G. Srama, R. Zook, H. A. TI Five years of Ulysses dust data: 2000-2004 SO PLANETARY AND SPACE SCIENCE LA English DT Article DE interplanetary dust; interstellar dust; dust streams; Lorentz force; Jupiter dust; zodiacal dust ID INNER SOLAR-SYSTEM; INTERSTELLAR DUST; METEOROID ENVIRONMENT; JOVIAN MAGNETOSPHERE; RADIATION PRESSURE; MASS-DISTRIBUTION; ASTEROID BELT; GALILEO; GRAINS; FLUX AB The Ulysses spacecraft has been orbiting the Sun on a highly inclined ellipse (i = 79 degrees, perihelion distance 1.3 AU, aphelion distance 5.4 AU) since it encountered Jupiter in 1992. Between January 2000 and December 2004, the spacecraft completed almost an entire revolution about the Sun, passing through perihelion in May 2001 and aphelion in July 2004. In this five-year period the dust detector on board recorded 4415 dust impacts. We publish and analyse the complete data set of both raw and reduced data for particles with masses 10(-16) g <= M <= 10(-7) g. Together with. 1695 dust impacts recorded between launch of Ulysses and the end of 1999 published earlier (Grain, E., Baguhl, M., Divine, N., Fechtig, H., Hamilton, D.P, Harmer, M.S., Kissel, J., Lindblad, B.A., Linkert, D., Linkert, G., Mann, L, McDonnell, J.A.M., Morfill, G.E., Polanskey, C., Riemann, R., Schwehm, G.H., Siddique, N., Staubach, P., Zook, H.A., 1995a. Two years of Ulysses dust data. Planetary Space Sci. 43, 971-999, Paper III; Kruger, H., Grun, E., Landgraf, M., Baguhl, M., Dermott, S.F., Fechtig, H., Gustafson, B.A., Hamilton, D.P., Harmer, M.S., Horanyi, M., Kissel, J., Lindblad, B., Linkert, D., Linkert, G., Mann, L, McDonnell, J.A.M., Morfill, G.E., Polanskey, C., Schwehm, G.H., Srama, R., Zook, H.A., 1995. Three years of Ulysses dust data: 1993 to 1995. Planetary and Space Sci. 47, 363-383, Paper V; Kruger, H., Grun, E., Landgraf, M., Dermott, S.F., Fechtig, H., Gustafson, B.A., Hamilton, D.P., Harmer, M.S., Horanyi, M., Kissel, J., Lindblad, B., Linkert, D., Linkert, G., Mann, I., McDonnell, J.A.M., Morfill, G.E., Polanskey, C., Schwehm, G.H., Srama, R., Zook, H.A., 2001b. Four years of Ulysses dust data: 1996 to 1999. Planetary Space Sci. 49, 1303-1324, Paper VII), a data set of 6110 dust impacts detected with the Ulysses sensor between October 1990 and December 2004 is now available. The impact rate measured between 2000 and 2002 was relatively constant with about 0.3 impacts per day showing a maximum at 1.5 per day around ecliptic plane crossing in early-2001. The impact direction of the majority of impacts between 2000 and 2002 is compatible with particles of interstellar origin, the rest are most likely interplanetary particles. In 2003 and 2004 dust stream particles originating from the jovian system dominated the overall impact rate. Twenty-two individual dust streams were measured between November 2002 and December 2004. The observed impact rates are compared with models for interplanetary and interstellar dust. The dust measurements from the entire mission since Ulysses launch give good agreement with the interplanetary flux model of Staubach, P., Grun, E., Jehn, R., 1997. The meteoroid environment near Earth, Adv. Space Res. 19, 301-308. (c) 2006 Elsevier Ltd. All rights reserved. C1 Max Planck Inst Sonnensystemforsch, D-37191 Katlenburg Lindau, Germany. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. Max Planck Inst Kernphys, D-69029 Heidelberg, Germany. Univ Florida, Gainesville, FL 32609 USA. CNR, ARTOV, INAF, Ist Fis Spazio Interplanetario, I-00133 Rome, Italy. Hawaii Inst Geophys & Planetol, Honolulu, HI 96822 USA. Univ Maryland, College Pk, MD 20742 USA. Univ Colorado, Atmospher & Space Phys Lab, Boulder, CO 80309 USA. ESOC, D-64293 Darmstadt, Germany. Lund Observ, S-221 Lund, Sweden. Univ Munster, Inst Planetol, D-48149 Munster, Germany. Open Univ, Planetary & Space Sci Res Inst, Milton Keynes MK7 6AA, Bucks, England. Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. ESTEC, NL-2200 AG Noordwijk, Netherlands. NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. RP Kruger, H (reprint author), Max Planck Inst Sonnensystemforsch, D-37191 Katlenburg Lindau, Germany. EM krueger@mps.mpg.de RI Gustafson, Bo/B-9526-2011; OI Horanyi, Mihaly/0000-0002-5920-9226 NR 60 TC 20 Z9 20 U1 1 U2 5 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0032-0633 J9 PLANET SPACE SCI JI Planet Space Sci. PD AUG PY 2006 VL 54 IS 9-10 BP 932 EP 956 DI 10.1016/j.pss.2006.04.015 PG 25 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 088BJ UT WOS:000240786200008 ER PT J AU Srama, R Kempf, S Moragas-Klostermeyer, G Helfert, S Ahrens, TJ Altobelli, N Auer, S Beckmann, U Bradley, JG Burton, M Dikarev, VV Economou, T Fechtig, H Green, SF Grande, M Havnes, O Hillier, JK Horanyi, M Igenbergs, E Jessberger, EK Johnson, TV Kruger, H Matt, G McBride, N Mocker, A Lamy, P Linkert, D Linkert, G Lura, F McDonnell, JAM Mohlmann, D Morfill, GE Postberg, F Roy, M Schwehm, GH Spahn, F Svestka, J Tschernjawski, V Tuzzolino, AJ Wasch, R Grun, E AF Srama, R. Kempf, S. Moragas-Klostermeyer, G. Helfert, S. Ahrens, T. J. Altobelli, N. Auer, S. Beckmann, U. Bradley, J. G. Burton, M. Dikarev, V. V. Economou, T. Fechtig, H. Green, S. F. Grande, M. Havnes, O. Hillier, J. K. Horanyi, M. Igenbergs, E. Jessberger, E. K. Johnson, T. V. Krueger, H. Matt, G. McBride, N. Mocker, A. Lamy, P. Linkert, D. Linkert, G. Lura, F. McDonnell, J. A. M. Moehlmann, D. Morfill, G. E. Postberg, F. Roy, M. Schwehm, G. H. Spahn, F. Svestka, J. Tschernjawski, V. Tuzzolino, A. J. Waesch, R. Gruen, E. TI In situ dust measurements in the inner Saturnian system SO PLANETARY AND SPACE SCIENCE LA English DT Article DE Cassini; dust; CDA; E-ring; water ice ID E-RING; PARTICLES; CASSINI; DYNAMICS AB In July 2004 the Cassini-Huygens mission reached the Saturnian system and started its orbital tour. A total of 75 orbits will be carried out during the primary mission until August 2008. In these four years Cassini crosses the ring plane 150 times and spends approx. 400 h within Titan's orbit. The Cosmic Dust Analyser (CDA) onboard Cassini characterises the dust environment with its extended E ring and embedded moons. Here, we focus on the CDA results of the first year and we present the Dust Analyser (DA) data within Titan's orbit. This paper does investigate High Rate Detector data and dust composition measurements. The authors focus on the analysis of impact rates, which were strongly variable primarily due to changes of the spacecraft pointing. An overview is given about the ring plane crossings and the DA counter measurements. The DA dust impact rates are compared with the DA boresight configuration around all ring plane crossings between June 2004 and July 2005. Dust impacts were registered at altitudes as high as 100 000 km above the ring plane at distances from Saturn between 4 and 10 Saturn radii. In those regions the dust density of particles bigger than 0.5 mu m can reach values of 0.001 m(-3). (c) 2006 Published by Elsevier Ltd. C1 Max Planck Inst Nucl Phys, Heidelberg, Germany. CALTECH, Seismol Lab, Pasadena, CA 91125 USA. CALTECH, Jet Prop Lab, Pasadena, CA USA. Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA. Open Univ, Milton Keynes MK7 6AA, Bucks, England. Rutherford Appleton Lab, Didcot OX11 0QX, Oxon, England. Univ Tromso, Auroral Observ, N-9001 Tromso, Norway. Univ Colorado, Boulder, CO 80309 USA. Tech Univ Munich, D-8046 Garching, Germany. Univ Munster, D-4400 Munster, Germany. Max Planck Inst Solar Syst Res, Katlenburg Lindau, Germany. Astron Spatiale Lab, Marseille, France. DLR, Berlin, Germany. Max Planck Inst Phys & Astron, Garching, Germany. ESA, Estec, Noordwijk, Netherlands. Univ Potsdam, Potsdam, Germany. Prague Observ, Prague, Czech Republic. Univ Hawaii, HIGP, Honolulu, HI 96822 USA. RP Srama, R (reprint author), Max Planck Inst Nucl Phys, Heidelberg, Germany. EM ralf.srama@mpi-hd.mpg.de RI Green, Simon/C-7408-2009; Grande, Manuel/C-2242-2013; OI Grande, Manuel/0000-0002-2233-2618; KEMPF, SASCHA/0000-0001-5236-3004; Horanyi, Mihaly/0000-0002-5920-9226 NR 20 TC 37 Z9 37 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 AUG PY 2006 VL 54 IS 9-10 BP 967 EP 987 DI 10.1016/j.pss.2006.05.021 PG 21 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 088BJ UT WOS:000240786200010 ER PT J AU Rednikov, AY Zhao, H Sadhal, SS Trinh, EH AF Rednikov, A. Y. Zhao, Hong Sadhal, S. S. Trinh, E. H. TI Steady streaming around a spherical drop displaced from the velocity antinode in an acoustic levitation field SO QUARTERLY JOURNAL OF MECHANICS AND APPLIED MATHEMATICS LA English DT Article ID RADIATION FORCE; VISCOUS-FLUID; TORSIONAL OSCILLATIONS; BUBBLE; CYLINDER; FLOW AB The steady (acoustic) streaming associated with a spherical drop displaced from the velocity antinode of a standing wave is studied. The ratio of the particle size to the acoustic wavelength is treated as small but non-zero, and the solution is developed in the form of a two-term expansion in terms of the corresponding smallness parameter. The drop viscosity is assumed to be much higher than that of the surrounding fluid, which is the case for a drop in a gas medium. There are essentially three distinct regions where the steady streaming flow is analysed: inside the drop (internal circulation), in the Stokes shear-wave layer at the surface on the gas side, and the gas outside the Stokes layer (the outer streaming region). Solutions for the internal circulation and the outer streaming are obtained in the limit of small Reynolds number. Despite the gas-to-liquid viscosity ratio being small, the outer streaming may be dramatically affected by the fact that the sphere is liquid as opposed to solid. The parameter that measures the effect of liquidity is essentially the viscosity ratio divided by the relative (to the particle size) thickness of the Stokes layer. The case of a solid sphere is recovered by letting this parameter go to zero. C1 Univ So Calif, Aerosp & Mech Engn, Los Angeles, CA 90089 USA. NASA Headquarters, Code UG, Washington, DC 20546 USA. RP Rednikov, AY (reprint author), Univ So Calif, Aerosp & Mech Engn, Los Angeles, CA 90089 USA. EM sadhal@usc.edu NR 30 TC 24 Z9 24 U1 1 U2 10 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0033-5614 J9 Q J MECH APPL MATH JI Q. J. Mech. Appl. Math. PD AUG PY 2006 VL 59 BP 377 EP 397 DI 10.1093/qjmam/hbl007 PN 3 PG 21 WC Mathematics, Applied; Mechanics SC Mathematics; Mechanics GA 074VR UT WOS:000239840400004 ER PT J AU Li, B Li, M Chen, K Smidts, C AF Li, Bin Li, Ming Chen, Ken Smidts, Carol TI Integrating software into PRA: A software-related failure mode taxonomy SO RISK ANALYSIS LA English DT Article DE failure modes; PRA; software; taxonomy AB Probabilistic risk assessment is a methodology to assess the probability of failure or success of a mission. Results provided by the risk assessment methodology are used to make decisions concerning choice of upgrades, scheduling of maintenance, decision to launch, etc. However, current PRA neglects the contribution of software to the risk of failure of the mission. Our research has developed a methodology to account for the impact of software to system failure. This article focuses on an element of the approach: a comprehensive taxonomy of software-related failure modes. Application of the taxonomy is discussed in this article. A validation of the taxonomy and conclusions drawn from this validation effort are described. Future research is also summarized. C1 Univ Maryland, Ctr Reliabil Engn, College Pk, MD 20742 USA. NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. RP Smidts, C (reprint author), Univ Maryland, Ctr Reliabil Engn, College Pk, MD 20742 USA. EM csmidts@eng.umd.edu NR 45 TC 4 Z9 4 U1 0 U2 2 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0272-4332 J9 RISK ANAL JI Risk Anal. PD AUG PY 2006 VL 26 IS 4 BP 997 EP 1012 DI 10.1111/j.1539-6924.2006.00795.x PG 16 WC Public, Environmental & Occupational Health; Mathematics, Interdisciplinary Applications; Social Sciences, Mathematical Methods SC Public, Environmental & Occupational Health; Mathematics; Mathematical Methods In Social Sciences GA 075PJ UT WOS:000239897400013 PM 16948692 ER PT J AU Storm, T AF Storm, T. TI How do space probes navigate large distances with such accuracy? SO SCIENTIFIC AMERICAN LA English DT Letter C1 NASA, Jet Prop Lab, Cassini Project, Washington, DC 20546 USA. RP Storm, T (reprint author), NASA, Jet Prop Lab, Cassini Project, 300 E St SW, Washington, DC 20546 USA. NR 0 TC 0 Z9 0 U1 0 U2 0 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 AUG PY 2006 VL 295 IS 2 BP 100 EP 100 PG 1 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 064TT UT WOS:000239112700040 ER PT J AU Tansel, B Sager, J Rector, T Garland, J Strayer, RF Levine, LF Roberts, M Hummerick, M Bauer, J AF Tansel, Berrin Sager, John Rector, Tony Garland, Jay Strayer, Richard F. Levine, Lanfang Roberts, Michael Hummerick, Mary Bauer, Jan TI Significance of hydrated radius and hydration shells on ionic permeability during nanofiltration in dead end and cross flow modes SO SEPARATION AND PURIFICATION TECHNOLOGY LA English DT Article DE nanofiltration; hydrated radius; ion permeability; dead end filtration; cross flow filtration ID MOLECULAR-DYNAMICS; MEMBRANES; WATER; MECHANISMS; SOLUTES; DENSITY; CAKE AB The aerobic rotational membrane system (ARMS) is one of the water recovery and recycling processes considered for use during long space missions. The ARMS effluent contains high levels of dissolved inorganic salts to be removed by the closed loop water recovery and recycling system. The purpose of this study was to investigate the permeability characteristics of ions present in the ARMS effluent through a nanofiltration membrane. Experiments were conducted in stirred dead end and cross flow filtration modes to evaluate the effectiveness of nanofiltration process to remove dissolved solids. The rejection characteristics of the ions were evaluated in relation to ionic hydrated radius, hydration number and ionic viscosity parameters. Permeability of ions through the nanofiltration membrane showed a strong correlation with their hydrated radii. The ions with relatively smaller crystal radii (i.e., Mg2+ and Ca2+) have higher hydration numbers and larger hydrated radii. These ions also hold their hydration shells more strongly, hence, they were removed by both filtration modes but more effectively by dead end filtration. On the other hand, the ions with larger crystal radii (i.e., K+ and Na+) have weaker hydration shells, hence, they may be able to detach from their hydration layer while passing through the nanofiltration membrane. In dead end mode, the ions are subjected to relatively larger shear forces to pass through the membrane in comparison to cross flow where the ions move parallel to the membrane surface, hence the shear force is reduced. The permeation of the ions was consistently higher in the dead end mode than the cross flow mode operated at the same pressure. (C) 2005 Elsevier B.V. All rights reserved. C1 Florida Int Univ, Dept Civil & Environm Engn, Miami, FL 33199 USA. NASA, Kennedy Space Ctr, FL USA. Dynamac Corp, Kennedy Space Ctr, FL USA. RP Tansel, B (reprint author), Florida Int Univ, Dept Civil & Environm Engn, Miami, FL 33199 USA. EM tanselb@fiu.edu NR 24 TC 137 Z9 153 U1 17 U2 121 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 1383-5866 J9 SEP PURIF TECHNOL JI Sep. Purif. Technol. PD AUG PY 2006 VL 51 IS 1 BP 40 EP 47 DI 10.1016/j.seppur.2005.12.020 PG 8 WC Engineering, Chemical SC Engineering GA 075IC UT WOS:000239877100006 ER PT J AU Sturrock, PA Scargle, JD AF Sturrock, P. A. Scargle, J. D. TI Power-spectrum analysis of super-kamiokande solar neutrino data, taking into account asymmetry in the error estimates SO SOLAR PHYSICS LA English DT Article ID ROTATING STARS; TIME-SERIES; FLUX; OSCILLATIONS; PERIODICITIES AB The purpose of this article is to carry out a power-spectrum analysis of the Super-Kamiokande five-day dataset that takes account of the asymmetry in the error estimates. Whereas for symmetrical error estimates the likelihood analysis involves a linear optimization procedure, for asymmetrical error estimates it involves a nonlinear optimization procedure. For most frequencies there is little difference between the power spectra derived from analyses of symmetrized error estimates and from asymmetrical error estimates, but this is not the case for the principal peak in the power spectrum at 9.43 yr(-1). A likelihood analysis that takes account of the error asymmetry leads to a peak with power 13.24 at that frequency, and a Monte Carlo analysis shows that there is a chance of only 0.1% of finding a peak this big or bigger in the search band 1 - 36 yr(-1). From this perspective, power-spectrum analysis that takes account of asymmetry of the error estimates gives evidence for variability that is significant at the 99.9% level. We comment briefly on an apparent discrepancy between power-spectrum analyses of the Super-Kamiokande and SNO solar neutrino experiments. C1 Stanford Univ, Ctr Space Sci & Astrophys, Stanford, CA 94305 USA. NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Sturrock, PA (reprint author), Stanford Univ, Ctr Space Sci & Astrophys, Varian 302, Stanford, CA 94305 USA. EM sturrock@stanford.edu; jeffrey@cosmic.arc.nasa.gov NR 29 TC 10 Z9 10 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 AUG PY 2006 VL 237 IS 1 BP 1 EP 11 DI 10.1007/s11207-006-0143-0 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 073HR UT WOS:000239734100001 ER PT J AU Moran, TG Davila, JM Morrill, JS Wang, D Howard, R AF Moran, Thomas G. Davila, Joseph M. Morrill, Jeff S. Wang, Dennis Howard, Russel TI Solar and heliospheric observatory/large angle spectrometric coronagraph polarimetric calibration SO SOLAR PHYSICS LA English DT Article ID LIGHT AB We present a polarimetric characterization and correction for the Solar and Heliospheric Observatory/Large Angle Spectrometric Coronagraph (SOHO/LASCO) C2 and C3 white light coronagraphs. By measuring the uncorrected polarization angles in solar minimum C2 coronal images, we have determined that the coronagraph acts as an optical phase retarder which converts a small fraction of the incoming radiation polarization from linear to circular. In addition, from the measurements of polarization angle in C3 coronal images we have determined that a component of the instrumentally scattered light in that instrument is polarized. We infer the retardation angle for C2 and compute the corresponding Mueller matrix, and determine the polarized stray light spatial profile in C3. The C2 Mueller matrix and C3 polarized stray light profiles are used to correct for instrumental effects in solar minimum coronal observations to obtain polarized brightness between two and thirty-two solar radii, which show deep polar coronal holes extending to the limit of the field of view. C1 Catholic Univ Amer, Washington, DC 20064 USA. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. USN, Res Lab, Div Space Sci, Washington, DC 20375 USA. RP Moran, TG (reprint author), Catholic Univ Amer, Washington, DC 20064 USA. EM moran@esa.nascom.nasa.gov; davila@lindsay.gsfc.nasa.gov; morrill@shogun.nrl; dennis.wang@nrl.navy.mil; russel.howard@nrl.navy.mil NR 10 TC 9 Z9 9 U1 2 U2 2 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0038-0938 J9 SOL PHYS JI Sol. Phys. PD AUG PY 2006 VL 237 IS 1 BP 211 EP 222 DI 10.1007/s11207-006-0147-9 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 073HR UT WOS:000239734100015 ER PT J AU McDanels, SJ AF McDanels, S. J. TI Space Shuttle Columbia post-accident analysis and investigation SO STRAIN LA English DT Article C1 NASA, Kennedy Space Ctr, FL 32899 USA. RP McDanels, SJ (reprint author), NASA, Kennedy Space Ctr, FL 32899 USA. NR 1 TC 0 Z9 0 U1 0 U2 2 PU BLACKWELL PUBLISHING PI OXFORD PA 9600 GARSINGTON RD, OXFORD OX4 2DQ, OXON, ENGLAND SN 0039-2103 J9 STRAIN JI Strain PD AUG PY 2006 VL 42 IS 3 BP 159 EP 163 DI 10.1111/j.1475-1305.2006.00275.x PG 5 WC Materials Science, Characterization & Testing SC Materials Science GA 077IG UT WOS:000240021900004 ER PT J AU DellaCorte, C AF DellaCorte, Christopher TI Finding needles in haystacks SO TRIBOLOGY & LUBRICATION TECHNOLOGY LA English DT Editorial Material C1 NASA, Glenn Res Ctr Cleveland, Cleveland, OH 44135 USA. RP DellaCorte, C (reprint author), NASA, Glenn Res Ctr Cleveland, Cleveland, OH 44135 USA. EM cdellacorte@stle.org NR 0 TC 1 Z9 1 U1 0 U2 0 PU SOC TRIBOLOGISTS & LUBRICATION ENGINEERS PI PARK RIDGE PA 840 BUSSE HIGHWAY, PARK RIDGE, IL 60068 USA SN 0024-7154 J9 TRIBOL LUBR TECHNOL JI Tribol. Lubr. Technol. PD AUG PY 2006 VL 62 IS 8 BP 6 EP 6 PG 1 WC Engineering, Mechanical SC Engineering GA 075TZ UT WOS:000239909400002 ER PT J AU Folk, CL Remington, R AF Folk, Charles L. Remington, Roger TI Top-down modulation of preattentive processing: Testing the recovery account of contingent capture SO VISUAL COGNITION LA English DT Article; Proceedings Paper CT Munich Visual Search Symposium CY JUN 06-10, 2003 CL Holzhausen, GERMANY ID ATTENTIONAL CONTROL SETTINGS; VISUAL-SEARCH; INHIBITION; RETURN; COLOR; SET; SELECTIVITY; SINGLETONS; FEATURES AB One highly controversial issue with respect to preattentive processing concerns the degree to which the preattentive detection of "singletons" elicits an involuntary shift of spatial attention (i.e., attentional capture) that is immune from top-down modulation. According to the "pure-capture" perspective, preattentive processing drives the allocation of spatial attention in a purely bottom-up manner, in order of relative salience. According to the "contingent-capture" perspective, preattentive processing can produce attentional capture, but such capture is contingent on whether the eliciting stimulus carries a feature property consistent with the current attentional set. Pure-capture proponents have recently argued that the evidence for contingencies in attentional capture actually reflects the rapid disengagement and recovery from capture. Two spatial cueing experiments tested the rapid recovery by measuring (1) compatibility effects associated with irrelevant distractors and (2) inhibition of return to irrelevant distractors. These two measures provide converging evidence against the rapid recovery account. C1 Villanova Univ, Ames Res Ctr, NASA, Dept Psychol, Villanova, PA 19085 USA. RP Folk, CL (reprint author), Villanova Univ, Ames Res Ctr, NASA, Dept Psychol, Villanova, PA 19085 USA. EM charles.folk@villanova.edu NR 25 TC 65 Z9 67 U1 3 U2 10 PU PSYCHOLOGY PRESS PI HOVE PA 27 CHURCH RD, HOVE BN3 2FA, EAST SUSSEX, ENGLAND SN 1350-6285 J9 VIS COGN JI Vis. Cogn. PD AUG-DEC PY 2006 VL 14 IS 4-8 BP 445 EP 465 DI 10.1080/13506280500193545 PG 21 WC Psychology, Experimental SC Psychology GA 077IE UT WOS:000240021700003 ER PT J AU Davies, S Mann, GW Carslaw, KS Chipperfield, MP Remedios, JJ Allen, G Waterfall, AM Spang, R Toon, GC AF Davies, S. Mann, G. W. Carslaw, K. S. Chipperfield, M. P. Remedios, J. J. Allen, G. Waterfall, A. M. Spang, R. Toon, G. C. TI Testing our understanding of Arctic denitrification using MIPAS-E satellite measurements in winter 2002/2003 SO ATMOSPHERIC CHEMISTRY AND PHYSICS LA English DT Article ID LARGE HNO3-CONTAINING PARTICLES; STRATOSPHERIC AEROSOLS; MICROPHYSICAL MODEL; POLAR VORTEX; OZONE LOSS; HNO3; NUCLEATION; CLOUDS; CRISTA; NAT AB Observations of gas-phase HNO3 and N2O in the polar stratosphere from the Michelson Interferometer for Passive Atmospheric Sounding aboard the ENVISAT satellite (MIPAS-E) were made during the cold Arctic winter of 2002/2003. Vortex temperatures were unusually low in early winter and remained favourable for polar stratospheric cloud formation and denitrification until mid-January. MIPAS-E observations provide the first dataset with sufficient coverage of the polar vortex in mid-winter which enables a reasonable estimate of the timing of onset and spatial distribution of denitrification of the Arctic lower stratosphere to be performed. We use the observations from MIPAS-E to test the evolution of denitrification in the DLAPSE (Denitrification by Lagrangian Particle Sedimentation) microphysical denitrification modelcoupled to the SLIMCAT chemical transport model. In addition, the predicted denitrification from a simple equilibrium nitric acid trihydrate-based scheme is also compared with MIPAS-E. Modelled denitrification is compared with in-vortex NOy and N2O observations from the balloon-borne MarkIV interferometer in mid-December. Denitrification was clearly observed by MIPAS-E in mid-December 2002 and reached 80% in the core of the vortex by early January 2003. The DLAPSE model is broadly able to capture both the timing of onset and the spatial distribution of the observed denitrification. A simple thermodynamic equilibrium scheme is able to reproduce the observed denitrification in the core of the vortex but overestimates denitrification closer to the vortex edge. This study also suggests that the onset of denitrification in simple thermodynamic schemes may be earlier than in the MIPAS-E observations. C1 Univ Leeds, Inst Atmospher Sci, Sch Earth & Environm, Leeds LS2 9JT, W Yorkshire, England. Univ Leicester, Space Res Ctr, Leicester LE1 7RH, Leics, England. Univ Manchester, Sch Earth Atmospher & Atmospher Sci, Manchester M13 9PL, Lancs, England. Rutherford Appleton Lab, Didcot OX11 0QX, Oxon, England. Forschungszentrum Julich, Inst Stratosphare 1, D-52425 Julich, Germany. CALTECH, Jet Prop Lab, Pasadena, CA USA. RP Davies, S (reprint author), Univ Leeds, Inst Atmospher Sci, Sch Earth & Environm, Leeds LS2 9JT, W Yorkshire, England. EM stewart@env.leeds.ac.uk RI Spang, Reinhold/A-2738-2013; Allen, Grant /A-7737-2013; Carslaw, Ken/C-8514-2009; Chipperfield, Martyn/H-6359-2013 OI Spang, Reinhold/0000-0002-2483-5761; Allen, Grant /0000-0002-7070-3620; Carslaw, Ken/0000-0002-6800-154X; Chipperfield, Martyn/0000-0002-6803-4149 NR 44 TC 7 Z9 7 U1 1 U2 2 PU COPERNICUS GESELLSCHAFT MBH PI GOTTINGEN PA BAHNHOFSALLEE 1E, GOTTINGEN, 37081, GERMANY SN 1680-7316 EI 1680-7324 J9 ATMOS CHEM PHYS JI Atmos. Chem. Phys. PD JUL 31 PY 2006 VL 6 BP 3149 EP 3161 PG 13 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 068YF UT WOS:000239410200001 ER PT J AU Takeda, H Yamaguchi, A Bogard, DD Karouji, Y Ebihara, M Ohtake, M Saiki, K Arai, T AF Takeda, Hiroshi Yamaguchi, A. Bogard, D. D. Karouji, Y. Ebihara, M. Ohtake, M. Saiki, K. Arai, T. TI Magnesian anorthosites and a deep crustal rock from the farside crust of the moon SO EARTH AND PLANETARY SCIENCE LETTERS LA English DT Article DE lunar meteorite; anorthosite; lunar farside; spinel troctolite; magma ocean ID EARLY LUNAR CRUST; METEORITES; SURFACE; CHRONOLOGY; EVOLUTION; GEOCHEMISTRY; PETROGENESIS; CATACLYSM; PETROLOGY; BRECCIAS AB Among over thirty lunar meteorites recovered from the hot deserts and Antarctica, Dhofar 489 is the most depleted in thorium (0.05 ppm), FeO, and rare earth elements (REE). Dhofar 489 is a crystalline matrix anorthositic breccia and includes clasts of magnesian anorthosites and a spine] troctolite. The Mg/(Mg+Fe) mol% (Mg numbers=75-85) of olivine and pyroxene grains in this meteorite are higher than those of the Apollo ferroan anorthosites. Such materials were not recovered by the Apollo and Luna missions. However, remote sensing data suggest that the estimated concentrations of Th and FeO are consistent with the presence of such samples on the farside of the Moon. The differentiation trend deduced from the mineralogy of the anorthositic clasts define a magnesian extension of the ferroan anorthosite (FAN) trend constructed from the Apollo samples. The presence of magnesian anorthositic clasts in Dhofar 489 still offers a possibility that the farside trend with magnesian compositions is more primitive than the FAN trend, and may require a revision of this classical differentiation trend. The Ar-Ar age of Dhofar 489 is 4.23 +/- 0.034 Gyr, which is older than most Ar ages reported for highland rocks returned by Apollo. The old Ar-Ar age of impact formation of this breccia and the presence of a fragment of spinel troctolite of deep crustal origin suggest that a basin forming event on the farside excavated the deep crust and magnesian anorthosites before formation of Imbrium. (c) 2006 Elsevier B.V. All rights reserved. C1 Chiba Inst Technol, Res Inst, Narashino, Chiba 2750016, Japan. Natl Inst Polar Res, Itabashi Ku, Tokyo 1738515, Japan. NASA, Lyndon B Johnson Space Ctr, ARES, Houston, TX 77058 USA. Tokyo Metropolitan Univ, Dept Chem, Tokyo 1930397, Japan. Japan Aerosp Explorat Agcy, Dept Planetary Sci, Sagamihara, Kanagawa 2298510, Japan. Osaka Univ, Grad Sch Sci, Dept Earth & Space Sci, Toyonaka, Osaka 5600043, Japan. RP Takeda, H (reprint author), Chiba Inst Technol, Res Inst, 3-17-1 Tsudanuma, Narashino, Chiba 2750016, Japan. EM takeda.hiroshi@it-chiba.ac.jp NR 47 TC 61 Z9 64 U1 0 U2 8 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 JUL 30 PY 2006 VL 247 IS 3-4 BP 171 EP 184 DI 10.1016/j.epsl.2006.04.004 PG 14 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 074PL UT WOS:000239824200001 ER PT J AU Bindlish, R Jackson, TJ Gasiewski, AJ Klein, M Njoku, EG AF Bindlish, Rajat Jackson, Thomas J. Gasiewski, Albin J. Klein, Marian Njoku, Eni G. TI Soil moisture mapping and AMSR-E validation using the PSR in SMEX02 SO REMOTE SENSING OF ENVIRONMENT LA English DT Article DE microwave remote sensing; soil moisture; AMSR; PSR ID MICROWAVE EMISSION; WATER-CONTENT; RETRIEVAL; SOYBEANS; CORN; GHZ AB Field experiments (SMEX02) were conducted to evaluate the effects of dense agricultural crop conditions on soil moisture retrieval using passive microwave remote sensing. Aircraft observations were collected using a new version of the Polarimetric Scanning Radiometer (PSR) that provided four C band and four X band frequencies. Observations were also available from the Aqua satellite Advanced Microwave Scanning Radiometer (AMSR-E) at these same frequencies. SMEX02 was conducted over a three-week period during the summer near Ames, Iowa. Corn and soybeans dominate the region. During the study period the corn was approaching its peak water content state and the soybeans were at the mid point of the growth cycle. Aircraft observations are compared to ground observations. Subsequently models are developed to describe the effects of corn and soybeans on soil moisture retrieval. Multiple altitude aircraft brightness temperatures were compared to AMSR-E observations to understand brightness temperature scaling and provide validation. The X-band observations from the two sensors were in reasonable agreement. The AMSR-E C-band observations were contaminated with anthropogenic RFI, which made comparison to the PSR invalid. Aircraft data along with ancillary data were used in a retrieval algorithm to map soil moisture. The PSR estimated soil moisture retrievals on a field-by-field comparison had a standard error of estimate (SEE) of 5.5%. The error reduced when high altitude soil moisture estimates were aggregated to 25 km resolution (same as AMSR-E EASE grid product resolution) (SEE similar to 2.85%). These soil moisture products provide a validation of the AMSR retrievals. PSR/CX soil moisture images show spatial and temporal patterns consistent with meteorological and soil conditions. The dynamic range of the PSR/CX observations indicates that reasonable soil moisture estimates can be obtained from AMSR, even in areas of high vegetation biomass content (similar to 4-8 kg/m2). (c) 2005 Elsevier Inc. All rights reserved. C1 USDA, ARS, SSAI, Hydrol & Remote Sensing Lab, Beltsville, MD 20705 USA. NOAA, Environm Technol Lab, Boulder, CO 80303 USA. Jet Propuls Lab, Pasadena, CA USA. RP Bindlish, R (reprint author), USDA, ARS, SSAI, Hydrol & Remote Sensing Lab, 104 Bldg,007 BARC W, Beltsville, MD 20705 USA. EM bindlish@hydrolab.arsusda.gov RI Xie, Xingmei/G-7311-2011 NR 20 TC 68 Z9 77 U1 2 U2 25 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 JUL 30 PY 2006 VL 103 IS 2 BP 127 EP 139 DI 10.1016/j.rse.2005.02.003 PG 13 WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic Technology SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science & Photographic Technology GA 068ID UT WOS:000239366000001 ER PT J AU Pinheiro, ACT Mahoney, R Privette, JL Tucker, CJ AF Pinheiro, A. C. T. Mahoney, R. Privette, J. L. Tucker, C. J. TI Development of a daily long term record of NOAA-14 AVHRR land surface temperature over Africa SO REMOTE SENSING OF ENVIRONMENT LA English DT Article DE land surface temperature; Advanced Very High Resolution Radiometer; Global Area Coverage; split window algorithm; Africa ID HIGH-RESOLUTION RADIOMETER; DIFFERENCE VEGETATION INDEX; ORBIT DRIFT; VALIDATION; PRODUCTS; CLASSIFICATION; EMISSIVITY; ALGORITHMS; CLIMATE; DATASET AB We developed a new 6-year daily, daytime and nighttime, NOAA-14 AVHRR based land surface temperature (LST) dataset over continental Africa for the period 1995 through 2000. The processing chain was developed within the Global Inventory Modeling and Mapping System (GIMMS) at NASA's Goddard Space Flight Center. This paper describes the processing methodology used to convert the Global Area Coverage Level-1b data into LST and collateral data layers, such as sun and view geometries, cloud mask, local time of observation, and latitude and longitude. We used the Ulivieri et al. [Ulivieri, C., M.M. Castronuovo, R. Francioni, and A. Cardillo (1994), A split window algorithm for estimating land surface temperature from satellites, Adv. Space Research, 14(3):59-65.] split window algorithm to determine LST values. This algorithm requires as input values of surface emissivity in AVHRR channels 4 and 5. Thus, we developed continental maps of emissivity using an ensemble approach that combines laboratory emissivity spectra, MODIS-derived maps of herbaceous and woody fractional cover, and the UNESCO FAO soil map. A preliminary evaluation of the resulting LST product over a savanna woodland in South Africa showed a bias of < 0.3 K and an uncertainty of < 1.3 K for daytime retrievals (< 2.5 K for night). More extensive validation is required before statistically significant uncertainties can be determined. The LST production chain described here could be adapted for any wide field of view sensor (e.g., MODIS, VIIRS), and the LST product may be suitable for monitoring spatial and temporal temperature trends, or as input to many process models (e.g., hydrological, ecosystem). (c) 2006 Elsevier Inc. All rights reserved. C1 NASA, Goddard Space Flight Ctr, Greenbelt, MD USA. Global Sci & Technol Inc, Greenbelt, MD USA. RP Pinheiro, ACT (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD USA. EM Ana.Pinheiro@gsfc.nasa.gov RI Privette, Jeffrey/G-7807-2011 OI Privette, Jeffrey/0000-0001-8267-9894 NR 43 TC 37 Z9 38 U1 0 U2 10 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 JUL 30 PY 2006 VL 103 IS 2 BP 153 EP 164 DI 10.1016/j.rse.2006.03.009 PG 12 WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic Technology SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science & Photographic Technology GA 068ID UT WOS:000239366000003 ER PT J AU Ozdogan, M Woodcock, CE AF Ozdogan, Mutlu Woodcock, Curtis E. TI Resolution dependent errors in remote sensing of cultivated areas SO REMOTE SENSING OF ENVIRONMENT LA English DT Article DE agriculture; variogram; IKONOS ID GLOBAL LAND-COVER; SPATIAL-RESOLUTION; AUTO-CORRELATION; DIGITAL IMAGES; SATELLITE DATA; FIELD SIZE; MODIS DATA; MODELS; CHINA; DISTRIBUTIONS AB Remote sensing has become a common and effective method for estimating the areal coverage of land cover classes. One class of particular interest is agriculture as area estimates of cultivated lands are important for purposes such as estimating yields or irrigation needs. The synoptic coverage of satellite imagery and the relative ease of automated analysis have led to widespread mapping of agriculture using remote sensing. The accuracy of area estimates derived from these maps is known to be related to the accuracy of the maps. However, even in the situation where the map is very accurate, errors in area estimates may occur. These errors result from the behavior of the distribution of subpixel proportions of cultivated areas, and how that behavior changes as a result of sensor spatial resolution and class definitions. The sensitivity of estimates of cultivated areas to sensor spatial resolution and to the choice of threshold used to define cultivated land is explored in six agriculturally distinct locations around the world. Using a beta model for the distribution of subpixel proportions that is parameterized using variograms, it is possible to model the distribution of subpixel proportions for any spatial resolution. When the spatial resolution is small with respect to the spatial structure of the landscape (as measured by the variogram range) use of any class definition threshold produces an estimate very close to the true area coverage. On the other hand, as the resolution becomes coarse in relation to the variogram range, the subpixel proportions are no longer concentrated at the extremes of the distribution and the difference between the estimated and the true area has greater sensitivity to the selected threshold used to define classes. Thus, for the cases examined here, both the resolution and the class definition threshold have a strong influence on area estimates. The spatial resolutions where errors can be large depend on landscape spatial structure, which can be quantified using variograms. The net effect is that for the same spatial resolution, some places will exhibit much larger errors in area estimates than others. For the site in the Anhui province of China, where agricultural fields are very small (0.07 ha on the average), area estimates are highly sensitive to class definition thresholds even at the relatively fine resolution of 45 in. Conversely, in California (USA) spatial resolutions as coarse as 500 m can be used to reliably estimate cultivated areas. Results also suggest that the proportion of the total area that is cultivated significantly influences the accuracy of area estimates. When the area proportion is low, the class definition threshold must also be low to achieve an accurate area estimate. Conversely, in areas dominated by agriculture, a very stringent class definition of cultivated lands is required for accurate area estimates. While explored in the context of estimation of cultivated areas, the findings presented here are generic to the problem of area estimation using remote sensing. (c) 2006 Elsevier Inc. All rights reserved. C1 NASA, Goddard Space Flight Ctr, Hydrol Sci Branch, Greenbelt, MD 20771 USA. Boston Univ, Dept Geog & Environm, Boston, MA 02215 USA. RP Ozdogan, M (reprint author), NASA, Goddard Space Flight Ctr, Hydrol Sci Branch, Code 614-3, Greenbelt, MD 20771 USA. EM ozdogan@hsb.gsfc.nasa.gov; curtis@bu.edu OI Ozdogan, Mutlu/0000-0002-1707-3375 NR 55 TC 57 Z9 61 U1 1 U2 19 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 JUL 30 PY 2006 VL 103 IS 2 BP 203 EP 217 DI 10.1016/j.rse.2006.04.004 PG 15 WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic Technology SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science & Photographic Technology GA 068ID UT WOS:000239366000007 ER PT J AU Holzer, M Primeau, FW AF Holzer, Mark Primeau, Francois W. TI The diffusive ocean conveyor SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID THERMOHALINE CIRCULATION; TRANSPORT; MODEL; LAYER; BELT AB We use a novel path-density transport diagnostic to trace out the deep branch of the ocean conveyor in a global circulation model. Our results suggest that the majority of the world's deep water is not transported back to the surface along the current systems of the standard great ocean conveyor (GOC). Standard GOC routes are evident only for waters with interior residence times, tau, less than about a thousand years, accounting for less than a quarter of the ventilation-to-re-exposure flux. Waters with longer t are spread across the deep oceans by the "diffusive conveyor" and, by tau similar to 3000 years, organized into a characteristic deep-North-Pacific pattern that is dominated by eddy diffusion. The observed depletion of oxygen and 14 C in the deep N Pacific is consistent with a diffusive conveyor and should not be interpreted as evidence of an advective terminus of the GOC deep branch. C1 NASA, Goddard Inst Space Studies, New York, NY 10025 USA. Columbia Univ, Dept Appl Phys & Appl Math, New York, NY USA. Univ British Columbia, Dept Earth & Ocean Sci, Vancouver, BC V5Z 1M9, Canada. Langara Coll, Dept Phys, Vancouver, BC, Canada. Univ Calif Irvine, Dept Earth Syst Sci, Irvine, CA 92697 USA. RP Holzer, M (reprint author), NASA, Goddard Inst Space Studies, 2880 Broadway, New York, NY 10025 USA. EM mholzer@eos.ubc.ca; fprimeau@uci.edu RI Primeau, Francois /A-7310-2011 OI Primeau, Francois /0000-0001-7452-9415 NR 21 TC 23 Z9 23 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 JUL 29 PY 2006 VL 33 IS 14 AR L14618 DI 10.1029/2006GL026232 PG 5 WC Geosciences, Multidisciplinary SC Geology GA 069ZO UT WOS:000239489400004 ER PT J AU Mishchenko, MI AF Mishchenko, Michael I. TI Radiative transfer in clouds with small-scale inhomogeneities: Microphysical approach SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID CORRELATED RANDOM MEDIUM; DROP-SIZE VARIABILITY; EXTINCTION; EQUATION; MODELS AB Several recent publications have indicated that cloud droplets belonging to a particular size range may tend to cluster by forming small random particle groups imbedded in an otherwise uniform cloud. To analyze radiative transfer in clouds with such small-scale inhomogeneities, we invoke the concepts of statistical electromagnetics. We show that as long as the assumptions of ergodicity and spatial uniformity hold, one can still apply the classical radiative transfer equation in which the participating extinction and phase matrices are obtained by averaging the respective single-particle matrices over all the particles constituting the cloud. This result implies that comparisons of in situ and remote-sensing retrievals of the cloud-particle size distribution can be problematic and should be performed with caution. 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 crmim@giss.nasa.gov RI Mishchenko, Michael/D-4426-2012 NR 17 TC 6 Z9 6 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 JUL 29 PY 2006 VL 33 IS 14 AR L14820 DI 10.1029/2006GL026312 PG 4 WC Geosciences, Multidisciplinary SC Geology GA 069ZO UT WOS:000239489400007 ER PT J AU Collins, WD Ramaswamy, V Schwarzkopf, MD Sun, Y Portmann, RW Fu, Q Casanova, SEB Dufresne, JL Fillmore, DW Forster, PMD Galin, VY Gohar, LK Ingram, WJ Kratz, DP Lefebvre, MP Li, J Marquet, P Oinas, V Tsushima, Y Uchiyama, T Zhong, WY AF Collins, W. D. Ramaswamy, V. Schwarzkopf, M. D. Sun, Y. Portmann, R. W. Fu, Q. Casanova, S. E. B. Dufresne, J. -L. Fillmore, D. W. Forster, P. M. D. Galin, V. Y. Gohar, L. K. Ingram, W. J. Kratz, D. P. Lefebvre, M. -P. Li, J. Marquet, P. Oinas, V. Tsushima, Y. Uchiyama, T. Zhong, W. Y. TI Radiative forcing by well-mixed greenhouse gases: Estimates from climate models in the Intergovernmental Panel on Climate Change (IPCC) Fourth Assessment Report (AR4) SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID GENERAL-CIRCULATION MODELS; CARBON-DIOXIDE; COOLING RATES; CODES; OZONE; ABSORPTION; ALGORITHM; AEROSOLS AB The radiative effects from increased concentrations of well-mixed greenhouse gases (WMGHGs) represent the most significant and best understood anthropogenic forcing of the climate system. The most comprehensive tools for simulating past and future climates influenced by WMGHGs are fully coupled atmosphere-ocean general circulation models (AOGCMs). Because of the importance of WMGHGs as forcing agents it is essential that AOGCMs compute the radiative forcing by these gases as accurately as possible. We present the results of a radiative transfer model intercomparison between the forcings computed by the radiative parameterizations of AOGCMs and by benchmark line-by-line (LBL) codes. The comparison is focused on forcing by CO2, CH4, N2O, CFC-11, CFC-12, and the increased H2O expected in warmer climates. The models included in the intercomparison include several LBL codes and most of the global models submitted to the Intergovernmental Panel on Climate Change (IPCC) Fourth Assessment Report (AR4). In general, the LBL models are in excellent agreement with each other. However, in many cases, there are substantial discrepancies among the AOGCMs and between the AOGCMs and LBL codes. In some cases this is because the AOGCMs neglect particular absorbers, in particular the near-infrared effects of CH4 and N2O, while in others it is due to the methods for modeling the radiative processes. The biases in the AOGCM forcings are generally largest at the surface level. We quantify these differences and discuss the implications for interpreting variations in forcing and response across the multimodel ensemble of AOGCM simulations assembled for the IPCC AR4. C1 Natl Ctr Atmospher Res, Climate & Global Dynam Div, Boulder, CO 80307 USA. Geophys Fluid Dynam Lab, Princeton, NJ 08542 USA. Natl Climate Ctr, CMA, Lab Climate Change, Beijing 100081, Peoples R China. NOAA, Aeron Lab, Boulder, CO 80305 USA. Univ Washington, Dept Atmospher Sci, Seattle, WA 98195 USA. Univ Reading, Dept Meteorol, Reading RG6 6BB, Berks, England. UPMC, CNRS, IPSL, LMD, F-75252 Paris 05, France. Lab Sci Climat & Environm, Gif Sur Yvette, France. Univ Leeds, Sch Earth & Environm, Leeds LS2 9JT, W Yorkshire, England. Russian Acad Sci, Inst Numer Math, Moscow 117333, Russia. Univ Oxford, Dept Phys, Clarendon Lab, Oxford OX1 3PU, England. NASA, Climate Sci Branch, Langley Res Ctr, Hampton, VA 23681 USA. Univ Victoria, Canadian Ctr Climate Modeling & Anal, Victoria, BC V8W 2Y2, Canada. CNRM, Meteo France, F-31057 Toulouse 01, France. NASA, Goddard Inst Space Studies, New York, NY 10025 USA. Japan Agcy Marine Earth Sci & Technol, Frontier Res Ctr Global Change, Kanazawa Ku, Yokohama, Kanagawa 2360001, Japan. Meteorol Res Inst, Tsukuba, Ibaraki 3050052, Japan. Univ London Imperial Coll Sci Technol & Med, Dept Phys, Space & Atmospher Phys Grp, London SW7 2BW, England. RP Collins, WD (reprint author), Natl Ctr Atmospher Res, Climate & Global Dynam Div, POB 3000, Boulder, CO 80307 USA. EM wcollins@ucar.edu; v.ramaswamy@noaa.gov; dan.schwarzkopf@noaa.gov; sunying@cma.gov.cn; robert.w.portmann@noaa.gov; qfu@atmos.washington.edu; s.e.b.casanova@reading.ac.uk; jean-louis.dufresne@lmd.jussieu.fr; david.fillmore@cea.fr; p.forster@see.leeds.ac.uk; galin@inm.ras.ru; sws01lkg@met.reading.ac.uk; ingram@atm.ox.ac.uk; david.p.kratz@nasa.gov; marie-pierre.lefebvre@lmd.jussieu.fr; jiangnan.li@ec.gc.ca; pascal.marquet@meteo.fr; voinas@giss.nasa.gov; tsussi@jamstec.go.jp; tuchiyam@mri-jma.go.jp; w.zhong@imperial.ac.uk RI Portmann, Robert/C-4903-2009; Collins, William/J-3147-2014; Dufresne, Jean-Louis/I-5616-2015; Li, Jiangnan/J-6262-2016; Forster, Piers/F-9829-2010; Manager, CSD Publications/B-2789-2015 OI Portmann, Robert/0000-0002-0279-6087; Collins, William/0000-0002-4463-9848; Dufresne, Jean-Louis/0000-0003-4764-9600; Forster, Piers/0000-0002-6078-0171; NR 45 TC 127 Z9 131 U1 1 U2 31 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 JUL 28 PY 2006 VL 111 IS D14 AR D14317 DI 10.1029/2005JD006713 PG 15 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 069ZT UT WOS:000239490100001 ER PT J AU Smirnov, A Holben, BN Sakerin, SM Kabanov, DM Slutsker, I Chin, M Diehl, TL Remer, LA Kahn, R Ignatov, A Liu, L Mishchenko, M Eck, TF Kucsera, TL Giles, D Kopelevich, OV AF Smirnov, A. Holben, B. N. Sakerin, S. M. Kabanov, D. M. Slutsker, I. Chin, M. Diehl, T. L. Remer, L. A. Kahn, R. Ignatov, A. Liu, L. Mishchenko, M. Eck, T. F. Kucsera, T. L. Giles, D. Kopelevich, O. V. TI Ship-based aerosol optical depth measurements in the Atlantic Ocean: Comparison with satellite retrievals and GOCART model SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID ATMOSPHERIC AEROSOL; SUN PHOTOMETER; WIND-SPEED; VALIDATION; THICKNESS; AERONET; DUST AB Aerosol optical depth measurements were made in October - December 2004 onboard the R/V Akademik Sergey Vavilov. The cruise area included an Atlantic transect from North Sea to Cape Town and then a crossing in the South Atlantic to Argentina. In the open oceanic areas not influenced by continental sources aerosol optical depth values were close to background oceanic conditions (tau(a) similar to 0.06 - 0.08). Spectral dependence, especially in the high latitude Southern Atlantic, can be considered as quasi-neutral ( Angstrom parameter a was less than 0.4). Back-trajectory analysis allowed statistical division of the aerosol optical parameters and showed similar properties for the North Atlantic polar marine, South Atlantic subtropical marine and South Atlantic polar marine air. Ship-borne aerosol optical depth comparisons to GOCART model and satellite retrievals revealed systematic biases. Satellite retrieved optical depths are generally higher by 0.02 - 0.07 ( depending on the sensor), especially in low tau(a) conditions. GOCART model simulated optical depths correlate well with the ship measurements and, despite overall bias and a notable disparity with the observations in a number of cases, about 30% agree within +/- 0.01. C1 Univ Maryland Baltimore Cty, Goddard Earth Sci & Technol Ctr, Baltimore, MD 21250 USA. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Russian Acad Sci, Siberian Branch, Inst Atmospher Opt, Tomsk, Russia. Sci Syst & Applicat Inc, Lanham, MD USA. CALTECH, Jet Prop Lab, Pasadena, CA USA. NOAA NESDIS, Off Res & Applicat, Camp Springs, MD USA. Columbia Univ, New York, NY USA. NASA, Goddard Inst Space Studies, New York, NY 10025 USA. Russian Acad Sci, Inst Oceanol, Moscow, Russia. RP Smirnov, A (reprint author), Univ Maryland Baltimore Cty, Goddard Earth Sci & Technol Ctr, Baltimore, MD 21250 USA. EM asmirnov@ltpmail.gsfc.nasa.gov; bholben@pop900.gsfc.nasa.gov; sms@iao.ru; ralph.kahn@jpl.nasa.gov; alex.ignatov@noaa.gov; lliu@giss.nasa.gov; mmishchenko@giss.nasa.gov; dgiles@ltpmailx.gsfc.nasa.gov; oleg@manta.sio.rssi.ru RI Ignatov, Alexander/F-5594-2010; Smirnov, Alexander/C-2121-2009; ECK, THOMAS/D-7407-2012; Chin, Mian/J-8354-2012; Kopelevich, Oleg/G-2248-2014; Kahn, Ralph/D-5371-2012; Mishchenko, Michael/D-4426-2012 OI Ignatov, Alexander/0000-0002-7463-5944; Smirnov, Alexander/0000-0002-8208-1304; Kopelevich, Oleg/0000-0002-3697-3387; Kahn, Ralph/0000-0002-5234-6359; NR 26 TC 36 Z9 38 U1 1 U2 6 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 JUL 27 PY 2006 VL 33 IS 14 AR L14817 DI 10.1029/2006GL026051 PG 4 WC Geosciences, Multidisciplinary SC Geology GA 069ZM UT WOS:000239489200003 ER PT J AU Kostiuk, T Livengood, TA Sonnabend, G Fast, KE Hewagama, T Murakawa, K Tokunaga, AT Annen, J Buhl, D Schmulling, F Luz, D Witasse, O AF Kostiuk, T. Livengood, T. A. Sonnabend, G. Fast, K. E. Hewagama, T. Murakawa, K. Tokunaga, A. T. Annen, J. Buhl, D. Schmuelling, F. Luz, D. Witasse, O. TI Stratospheric global winds on Titan at the time of Huygens descent SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Article ID HETERODYNE SPECTROSCOPY; ETHANE ABUNDANCE; ZONAL WINDS; ATMOSPHERE; DYNAMICS; TEMPERATURE; PROBE; PLANETS; CLOUDS AB [1] Measurements of stratospheric zonal winds on Titan were made in preparation for and during the time of the descent of the Huygens Probe into Titan's atmosphere on 14 January 2005. Fully resolved emission lines from ethane near 11.7 mu m were measured on the east, center, and west positions on Titan using the NASA/GSFC Heterodyne Instrument for Planetary Wind And Composition, HIPWAC, mounted on the National Astronomical Observatory of Japan 8.2 m Subaru Telescope on Mauna Kea, Hawaii. Analysis of the Doppler shifts of the emission line shapes yielded mean prograde gas velocity similar to 60 +/- 65 m/s at altitudes below similar to 120 km ( similar to 5 mbar). This result is consistent with retrievals from the Huygens Doppler Wind Experiment and from other observations near this altitude range. Current spectral line shapes, however, differed significantly from those obtained in similar measurements on Subaru in 2004 and on the NASA IRTF in 1993 1996, which retrieved prograde zonal winds 190 +/- 90 m/s at 230 km ( similar to 0.4 mbar). The cores of the emission lines, which probe the high-altitude region, could not be fitted as before to retrieve wind directly using the accepted atmospheric model for Titan. They imply an approximately tenfold increase in ethane mole fraction (1.2 x 10(-4)) with strong wind shear above the stratopause, providing a potential probe of the lower mesosphere and possible evidence of temporal and spatial variability. Results contribute to coordinated measurements of winds by various techniques providing information on the altitude distribution of wind velocity in Titan's atmosphere from near the surface to the lower mesosphere. C1 NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Univ Space Res Assoc, Washington, DC USA. Univ Cologne, Inst Phys 1, D-50937 Cologne, Germany. Univ Maryland, Dept Astron, College Pk, MD 20742 USA. Max Planck Inst Radioastron, D-53121 Bonn, Germany. Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. Observ Astron Lisboa, Lisbon, Portugal. Observ Paris, LESIA, F-75014 Paris, France. European Space Agcy, ESTEC, Res & Sci Support Dept, NL-2200 AG Noordwijk, Netherlands. RP Kostiuk, T (reprint author), NASA, Goddard Space Flight Ctr, Code 693, Greenbelt, MD 20771 USA. EM kostiuk@gsfc.nasa.gov RI Livengood, Timothy/C-8512-2012; Hewagama, T/C-8488-2012; Luz, David/J-4588-2013; Kostiuk, Theodor/A-3077-2014 OI Luz, David/0000-0002-9473-8035; NR 37 TC 12 Z9 12 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-PLANET JI J. Geophys. Res.-Planets PD JUL 27 PY 2006 VL 111 IS E7 AR E07S03 DI 10.1029/2005JE002630 PG 9 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 069ZZ UT WOS:000239490800001 ER PT J AU Witasse, O Lebreton, JP Bird, MK Dutta-Roy, R Folkner, WM Preston, RA Asmar, SW Gurvits, LI Pogrebenko, SV Avruch, IM Campbell, RM Bignall, HE Garrett, MA van Langevelde, HJ Parsley, SM Reynolds, C Szomoru, A Reynolds, JE Phillips, CJ Sault, RJ Tzioumis, AK Ghigo, F Langston, G Brisken, W Romney, JD Mujunen, A Ritakari, J Tingay, SJ Dodson, RG van't Klooster, CGM Blancquaert, T Coustenis, A Gendron, E Sicardy, B Hirtzig, M Luz, D Negrao, A Kostiuk, T Livengood, TA Hartung, M de Pater, I Adamkovics, M Lorenz, RD Roe, H Schaller, E Brown, M Bouchez, AH Trujillo, CA Buratti, BJ Caillault, L Magin, T Bourdon, A Laux, C AF Witasse, Olivier Lebreton, Jean-Pierre Bird, Michael K. Dutta-Roy, Robindro Folkner, William M. Preston, Robert A. Asmar, Sami W. Gurvits, Leonid I. Pogrebenko, Sergei V. Avruch, Ian M. Campbell, Robert M. Bignall, Hayley E. Garrett, Michael A. van Langevelde, Huib Jan Parsley, Stephen M. Reynolds, Cormac Szomoru, Arpad Reynolds, John E. Phillips, Chris J. Sault, Robert J. Tzioumis, Anastasios K. Ghigo, Frank Langston, Glen Brisken, Walter Romney, Jonathan D. Mujunen, Ari Ritakari, Jouko Tingay, Steven J. Dodson, Richard G. van't Klooster, C. G. M. Blancquaert, Thierry Coustenis, Athena Gendron, Eric Sicardy, Bruno Hirtzig, Mathieu Luz, David Negrao, Alberto Kostiuk, Theodor Livengood, Timothy A. Hartung, Markus de Pater, Imke Adamkovics, Mate Lorenz, Ralph D. Roe, Henry Schaller, Emily Brown, Michael Bouchez, Antonin H. Trujillo, Chad A. Buratti, Bonnie J. Caillault, Lise Magin, Thierry Bourdon, Anne Laux, Christophe TI Overview of the coordinated ground-based observations of Titan during the Huygens mission SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Article ID RADIO TRACKING; DIFFERENTIAL VLBI; MU-M; WINDS; ATMOSPHERE; SURFACE; PROBE; DYNAMICS; BALLOONS; DESCENT AB [ 1] Coordinated ground-based observations of Titan were performed around or during the Huygens atmospheric probe mission at Titan on 14 January 2005, connecting the momentary in situ observations by the probe with the synoptic coverage provided by continuing ground-based programs. These observations consisted of three different categories: ( 1) radio telescope tracking of the Huygens signal at 2040 MHz, ( 2) observations of the atmosphere and surface of Titan, and ( 3) attempts to observe radiation emitted during the Huygens Probe entry into Titan's atmosphere. The Probe radio signal was successfully acquired by a network of terrestrial telescopes, recovering a vertical profile of wind speed in Titan's atmosphere from 140 km altitude down to the surface. Ground-based observations brought new information on atmosphere and surface properties of the largest Saturnian moon. No positive detection of phenomena associated with the Probe entry was reported. This paper reviews all these measurements and highlights the achieved results. The ground-based observations, both radio and optical, are of fundamental importance for the interpretation of results from the Huygens mission. C1 European Space Agcy, ESTEC, Res & Sci Support Dept, NL-2200 AG Noordwijk, Netherlands. Univ Bonn, Inst Radioastron, D-53125 Bonn, Germany. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. Joint Inst VLBI Europe, NL-7990 AA Dwingeloo, Netherlands. CSIRO, Australia Telescope Natl Facil, Epping, NSW 1710, Australia. Natl Radio Astron Observ, Green Bank, WV 24944 USA. Natl Radio Astron Observ, Socorro, NM 87801 USA. Helsinki Univ Technol, Metsahovi Radio Observ, FIN-02540 Kylmala, Finland. Swinburne Univ Technol, Hawthorn, Vic 3122, Australia. Observ Astron Nacl, Alcala De Henares 28803, Spain. European Space Agcy, ESTEC, TEC Directorate, NL-2200 AG Noordwijk, Netherlands. Observ Paris, LESIA, F-92195 Meudon, France. Lab Planetol & Geodynam, Nantes, France. Observ Astron Lisboa, Lisbon, Portugal. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Natl Ctr Earth & Space Sci Educ, Washington, DC 20036 USA. European So Observ, Santiago 19, Chile. Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA. CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. CALTECH, Caltech Opt Observ, Pasadena, CA 91125 USA. Gemini Observ, Hilo, HI 96720 USA. Ecole Cent Paris, Lab EM2C, CNRS, UPR288, F-92295 Chatenay Malabry, France. RP Witasse, O (reprint author), European Space Agcy, ESTEC, Res & Sci Support Dept, NL-2200 AG Noordwijk, Netherlands. RI Livengood, Timothy/C-8512-2012; Tingay, Steven/B-5271-2013; Reynolds, Cormac/B-5635-2013; Bignall, Hayley/B-2867-2013; Luz, David/J-4588-2013; Kostiuk, Theodor/A-3077-2014; bourdon, anne/O-9869-2014; Magin, Thierry/A-7533-2016; Lorenz, Ralph/B-8759-2016; OI Reynolds, Cormac/0000-0002-8978-0626; Bignall, Hayley/0000-0001-6247-3071; Luz, David/0000-0002-9473-8035; bourdon, anne/0000-0003-3662-4651; Magin, Thierry/0000-0002-4376-1518; Lorenz, Ralph/0000-0001-8528-4644; Negrao, Alberto/0000-0001-6042-1294; van Langevelde, Huib Jan/0000-0002-0230-5946 NR 50 TC 12 Z9 12 U1 1 U2 1 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 JUL 27 PY 2006 VL 111 IS E7 AR E07S01 DI 10.1029/2005JE002640 PG 12 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 069ZZ UT WOS:000239490800002 ER PT J AU Tokano, T Mckay, CP Neubauer, FM Atreya, SK Ferri, F Fulchignoni, M Niemann, HB AF Tokano, Tetsuya McKay, Christopher P. Neubauer, Fritz M. Atreya, Sushil K. Ferri, Francesca Fulchignoni, Marcello Niemann, Hasso B. TI Methane drizzle on Titan SO NATURE LA English DT Article ID MIDLATITUDE CLOUDS; SOUTH-POLE; TROPOSPHERE; ATMOSPHERE; ABUNDANCES; SURFACE; WINDS; RAIN AB Saturn's moon Titan shows landscapes with fluvial features(1) suggestive of hydrology based on liquid methane. Recent efforts in understanding Titan's methane hydrological cycle have focused on occasional cloud outbursts near the south pole(2-4) or cloud streaks at southern mid-latitudes(5,6) and the mechanisms of their formation. It is not known, however, if the clouds produce rain or if there are also non-convective clouds, as predicted by several models(7-11). Here we show that the in situ data on the methane concentration and temperature profile in Titan's troposphere point to the presence of layered optically thin stratiform clouds. The data indicate an upper methane ice cloud and a lower, barely visible, liquid methane-nitrogen cloud, with a gap in between. The lower, liquid, cloud produces drizzle that reaches the surface. These non-convective methane clouds are quasi-permanent features supported by the global atmospheric circulation, indicating that methane precipitation occurs wherever there is slow upward motion. This drizzle is a persistent component of Titan's methane hydrological cycle and, by wetting the surface on a global scale, plays an active role in the surface geology of Titan. C1 Univ Cologne, Inst Geophys & Meteorol, D-50923 Cologne, Germany. NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA. Univ Padua, CISAS G Colombo, I-35131 Padua, Italy. Observ Paris, LESIA, F-92195 Meudon, France. Univ Paris 07, UFR Phys, F-75006 Paris, France. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20742 USA. RP Tokano, T (reprint author), Univ Cologne, Inst Geophys & Meteorol, Albertus Magnus Pl, D-50923 Cologne, Germany. EM tokano@geo.uni-koeln.de NR 30 TC 110 Z9 110 U1 0 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 JUL 27 PY 2006 VL 442 IS 7101 BP 432 EP 435 DI 10.1038/nature04948 PG 4 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 067CI UT WOS:000239278900038 PM 16871213 ER PT J AU Olsen, MA Douglass, AR Stolarski, RS Schoeberl, MR AF Olsen, Mark A. Douglass, Anne R. Stolarski, Richard S. Schoeberl, Mark R. TI On detecting a trend in the residual circulation from observations of column HCl SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID HALOGEN OCCULTATION EXPERIMENT; STRATOSPHERIC OZONE; TRANSPORT MODEL; MASS-EXCHANGE; ART.; TROPOSPHERE; CLIMATE; TROPOPAUSE; SPECTRA AB Ground-based measurements show that the HCl column at middle latitudes varies seasonally with a late spring maximum and a minimum in late summer. HALOE measurements of HCl profiles show that this seasonal cycle in the column is controlled by the seasonal variations of the mass and composition of the lowermost stratosphere. The seasonal maxima are produced by wintertime downward transport of stratospheric air. We hypothesize that the amplitude of the seasonal cycle is quantitatively related to the strength of the stratospheric residual circulation and stratosphere-troposphere exchange (STE). We investigate this relationship using a multi-decadal simulation from the GSFC Chemistry and Transport Model driven by output from a general circulation model in which an STE trend exists. We also examine the ground-based record of HCl measurements at Jungfraujoch for evidence of a trend in the HCl seasonal amplitude that would be a signature of a long-term change in the stratospheric circulation. C1 Univ Maryland Baltimore Cty, Goddard Earth Sci & Technol Ctr, Catonsville, MD 21228 USA. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Olsen, MA (reprint author), Univ Maryland Baltimore Cty, Goddard Earth Sci & Technol Ctr, Catonsville, MD 21228 USA. EM olsen@code613-3.gsfc.nasa.gov RI Douglass, Anne/D-4655-2012; Stolarski, Richard/B-8499-2013 OI Stolarski, Richard/0000-0001-8722-4012 NR 18 TC 1 Z9 1 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 JUL 26 PY 2006 VL 33 IS 14 AR L14815 DI 10.1029/2006GL026214 PG 5 WC Geosciences, Multidisciplinary SC Geology GA 069ZL UT WOS:000239489100005 ER PT J AU Shia, RL Liang, MC Miller, CE Yung, YL AF Shia, Run-Lie Liang, Mao-Chang Miller, Charles E. Yung, Yuk L. TI CO(2) in the upper troposphere: Influence of stratosphere-troposphere exchange SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID CARBON-DIOXIDE; NITROUS-OXIDE; TRANSPORT; VARIABILITY; SENSITIVITY; TROPOPAUSE; SCIAMACHY; METHANE; MODELS; RATIOS AB A two-dimensional transport model constrained to measured surface CO(2) concentrations was used to simulate the spatial and temporal variation of CO(2) in the atmosphere for the period from 1975 to 2004. We find that the amplitude, phase and shape of the CO(2) seasonal cycle vary as a function of both altitude and latitude. Cross tropopause exchanges, especially the downward branch of the Brewer-Dobson circulation, which brings stratospheric air to the upper troposphere at middle and high latitudes, change the CO(2) concentration and seasonal cycle in the extra-tropics. The model results match recent aircraft measurements of CO(2) in the upper troposphere (Matsueda et al., 2002) remarkably well. We conclude that upper tropospheric CO(2) volume mixing ratios will provide a valuable tool for validating vertical transport. The implications of the CO(2) variation caused by the stratosphere-troposphere exchange for remote sensing of CO(2) are discussed. C1 CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Shia, RL (reprint author), CALTECH, Div Geol & Planetary Sci, Mail Stop 150-21, Pasadena, CA 91125 USA. EM rls@gps.caltech.edu NR 27 TC 23 Z9 23 U1 1 U2 5 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD JUL 26 PY 2006 VL 33 IS 14 AR L14814 DI 10.1029/2006GL026141 PG 4 WC Geosciences, Multidisciplinary SC Geology GA 069ZL UT WOS:000239489100004 ER PT J AU Edwards, DP Emmons, LK Gille, JC Chu, A Attie, JL Giglio, L Wood, SW Haywood, J Deeter, MN Massie, ST Ziskin, DC Drummond, JR AF Edwards, D. P. Emmons, L. K. Gille, J. C. Chu, A. Attie, J. -L. Giglio, L. Wood, S. W. Haywood, J. Deeter, M. N. Massie, S. T. Ziskin, D. C. Drummond, J. R. TI Satellite-observed pollution from Southern Hemisphere biomass burning SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID INITIATIVE SAFARI 2000; RESOLUTION IMAGING SPECTRORADIOMETER; TROPOSPHERE MOPITT INSTRUMENT; AFRICAN SAVANNA ECOSYSTEMS; AEROSOL OPTICAL-THICKNESS; CARBON-MONOXIDE; TROPICAL ATLANTIC; TRACE GASES; DRY SEASON; ATMOSPHERIC CHEMISTRY AB [1] Biomass burning is a major source of pollution in the tropical Southern Hemisphere, and fine mode carbonaceous particles are produced by the same combustion processes that emit carbon monoxide ( CO). In this paper we examine these emissions with data from the Terra satellite, CO profiles from the Measurement of Pollution in the Troposphere (MOPITT) instrument, and fine-mode aerosol optical depth (AOD) from the Moderate-Resolution Imaging Spectroradiometer ( MODIS). The satellite measurements are used in conjunction with calculations from the MOZART chemical transport model to examine the 2003 Southern Hemisphere burning season with particular emphasis on the months of peak fire activity in September and October. Pollutant emissions follow the occurrence of dry season fires, and the temporal variation and spatial distributions of MOPITT CO and MODIS AOD are similar. We examine the outflow from Africa and South America with emphasis on the impact of these emissions on clean remote regions. We present comparisons of MOPITT observations and ground-based interferometer data from Lauder, New Zealand, which indicate that intercontinental transport of biomass burning pollution from Africa often determines the local air quality. The correlation between enhancements of AOD and CO column for distinct biomass burning plumes is very good with correlation coefficients greater than 0.8. We present a method using MOPITT and MODIS data for estimating the emission ratio of aerosol number density to CO concentration which could prove useful as input to modeling studies. We also investigate decay of plumes from African fires following export into the Indian Ocean and compare the MOPITT and MODIS measurements as a way of estimating the regional aerosol lifetime. Vertical transport of biomass burning emissions is also examined using CO profile information. Low-altitude concentrations are very high close to source regions, but further downwind of the continents, vertical mixing takes place and results in more even CO vertical distributions. In regions of significant convection, particularly in the equatorial Indian Ocean, the CO mixing ratio is greater at higher altitudes, indicating vertical transport of biomass burning emissions to the upper troposphere. C1 Natl Ctr Atmospher Res, Boulder, CO 80307 USA. Univ Maryland Baltimore Cty, Joint Ctr Earth Syst Technol, Baltimore, MD USA. Observ Midi Pyrenees, F-31400 Toulouse, France. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Natl Inst Water & Atmospher Res Ltd, Lauder, Cent Otago, New Zealand. Met Off, Exeter, Devon, England. Univ Toronto, Dept Phys, Toronto, ON, Canada. RP Edwards, DP (reprint author), Natl Ctr Atmospher Res, POB 3000, Boulder, CO 80307 USA. EM edwards@ucar.edu; emmons@ucar.edu; gille@ucar.edu; achu@climate.gsfc.nasa.gov; attjl@aero.obs-mip.fr; giglio@hades.gsfc.nasa.gov; s.wood@niwa.co.nz; jim.haywood@metoffice.gov.uk; mnd@ucar.edu; massie@ucar.edu; ziskin@ucar.edu; james.drummond@utoronto.ca RI Drummond, James/O-7467-2014; Deeter, Merritt/O-6078-2016; Emmons, Louisa/R-8922-2016 OI Deeter, Merritt/0000-0002-3555-0518; Emmons, Louisa/0000-0003-2325-6212 NR 87 TC 122 Z9 124 U1 0 U2 23 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X EI 2169-8996 J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD JUL 26 PY 2006 VL 111 IS D14 AR D14312 DI 10.1029/2005JD006655 PG 17 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 069ZR UT WOS:000239489700005 ER PT J AU Redemann, J Pilewskie, P Russell, PB Livingston, JM Howard, S Schmid, B Pommier, J Gore, W Eilers, J Wendisch, M AF Redemann, Jens Pilewskie, Peter Russell, Philip B. Livingston, John M. Howard, Steve Schmid, Beat Pommier, John Gore, Warren Eilers, James Wendisch, Manfred TI Airborne measurements of spectral direct aerosol radiative forcing in the Intercontinental chemical Transport Experiment/Intercontinental Transport and Chemical Transformation of anthropogenic pollution, 2004 SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID OCEAN EXPERIMENT INDOEX; OPTICAL-DEPTH; SURFACE; DISTRIBUTIONS; CLOSURE; TARFOX; COLUMN AB [ 1] As part of the INTEX-NA ( Intercontinental chemical Transport Experiment - North America) and ITCT ( Intercontinental Transport and Chemical Transformation of anthropogenic pollution) field studies, the NASA Ames 14-channel Airborne Tracking Sunphotometer (AATS-14) and a pair of Solar Spectral Flux Radiometers (SSFR) took measurements from aboard a Sky Research Jet stream 31 (J31) aircraft during 19 science flights over the Gulf of Maine during 12 July to 8 August 2004. The combination of coincident AATS-14 and SSFR measurements yields plots of net (downwelling minus upwelling) spectral irradiance as a function of aerosol optical depth (AOD) as measured along horizontal flight legs. By definition, the slope of these plots yields the instantaneous change in net irradiance per unit AOD change and is referred to as the instantaneous spectral aerosol radiative forcing efficiency, E-i ( W m(-2) nm(-1)). Numerical integration over a given spectral range yields the instantaneous broadband aerosol radiative forcing efficiency ( W m(-2)). This technique for deriving Ei is called the aerosol gradient method. Within 10 case studies considered suitable for our analysis we found a high variability in the derived instantaneous aerosol forcing efficiencies for the visible wavelength range ( 350 - 700 nm), with a mean of - 79.6 W m(-2) and a standard deviation of 21.8 W m(-2) (27%). An analytical conversion of the instantaneous forcing efficiencies to 24-hour-average values yielded - 45.8 +/- 13.1 W m(-2) (mean +/- std). We present spectrally resolved aerosol forcing efficiencies between 350 and 1670 nm, estimates of the midvisible aerosol single scattering albedo and a comparison of observed broadband forcing efficiencies to previously reported values. C1 Bay Area Environm Res Inst, Sonoma, CA 93003 USA. Univ Colorado, Atmospher & Space Phys Lab, Boulder, CO 80309 USA. NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. SRI Int, Menlo Pk, CA 94025 USA. Leibniz Inst Tropospher Res, Leipzig, Germany. RP Redemann, J (reprint author), Bay Area Environm Res Inst, Sonoma, CA 93003 USA. EM jredemann@mail.arc.nasa.gov RI Wendisch, Manfred/E-4175-2013 OI Wendisch, Manfred/0000-0002-4652-5561 NR 24 TC 20 Z9 20 U1 0 U2 4 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD JUL 26 PY 2006 VL 111 IS D14 AR D14210 DI 10.1029/2005JD006812 PG 10 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 069ZR UT WOS:000239489700008 ER PT J AU Capadona, LA Meador, MAB Alunni, A Fabrizio, EF Vassilaras, P Leventis, N AF Capadona, Lynn A. Meador, Mary Ann B. Alunni, Antonella Fabrizio, Eve F. Vassilaras, Plousia Leventis, Nicholas TI Flexible, low-density polymer crosslinked silica aerogels SO POLYMER LA English DT Article DE polymer crosslinked aerogels; mesoporous; di-isocyanates ID SOL AB Polymerization of a di-isocyanate with the amine-modified surface of a sol-gel derived mesoporous silica network crosslinks the nanoparticles of the silica skeleton, and reinforces the otherwise fragile framework. Systematically adjusting the processing variables affecting density produce aerogels whose macroscopic properties could be controlled, and are attributed to changing nanoscale morphology. Aerogels crosslinked using the smallest amount of silica studied exhibit as much as a 40-fold increase in strength over the corresponding non-crosslinked framework, and are flexible. (c) 2006 Elsevier Ltd. All rights reserved. C1 NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. RP Meador, MAB (reprint author), NASA, Glenn Res Ctr, 21000 Brookpk Rd, Cleveland, OH 44135 USA. EM maryann.meador@nasa.gov OI Meador, Mary Ann/0000-0003-2513-7372 NR 18 TC 67 Z9 74 U1 4 U2 55 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 JUL 26 PY 2006 VL 47 IS 16 BP 5754 EP 5761 DI 10.1016/j.polymer.2006.05.073 PG 8 WC Polymer Science SC Polymer Science GA 071QL UT WOS:000239616600007 ER PT J AU Clancy, TC Gates, TS AF Clancy, Thomas C. Gates, Thomas S. TI Modeling of interfacial modification effects on thermal conductivity of carbon nanotube composites SO POLYMER LA English DT Article DE nanocomposite; simulation; polymers ID HEAT-FLOW; RESISTANCE; DEPENDENCE AB The effect of functionalization of carbon nanotubes on the thermal conductivity of nanocomposites has been studied using a multi-scale modeling approach. These results predict that grafting linear hydrocarbon chains to the surface of a single wall carbon nanotube with covalent chemical bonds should result in a significant increase in the thermal conductivity of these nanocomposites. This is due to the decrease in the interfacial thermal (Kapitza) resistance between the single wall carbon nanotube and the surrounding polymer matrix upon chemical functionalization. The nanocomposites studied here consist of single wall carbon nanotubes in a bulk poly(ethylene vinyl acetate) matrix. The nanotubes are functionalized by end-grafting linear hydrocarbon chains of varying length to the surface of the nanotube. The effect which this functionalization has on the interfacial thermal resistance is studied by molecular dynamics simulation. Interfacial thermal resistance values are calculated for a range of chemical grafting densities and with several chain lengths. These results are subsequently used in an analytical model to predict the resulting effect on the bulk thermal conductivity of the nanocomposite. (c) 2006 Elsevier Ltd. All rights reserved. C1 Natl Inst Aerosp, Hampton, VA 23666 USA. NASA, Langley Res Ctr, Mech Struct & Mat Branch, Hampton, VA 23681 USA. RP Clancy, TC (reprint author), Natl Inst Aerosp, 100 Explorat Way, Hampton, VA 23666 USA. EM tclancy@nianet.org NR 17 TC 122 Z9 125 U1 2 U2 57 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 JUL 26 PY 2006 VL 47 IS 16 BP 5990 EP 5996 DI 10.1016/j.polymer.2006.05.062 PG 7 WC Polymer Science SC Polymer Science GA 071QL UT WOS:000239616600033 ER PT J AU Warneke, T Meirink, JF Bergamaschi, P Grooss, JU Notholt, J Toon, GC Velazco, V Goede, APH Schrems, O AF Warneke, T. Meirink, J. F. Bergamaschi, P. Grooss, J. -U. Notholt, J. Toon, G. C. Velazco, V. Goede, A. P. H. Schrems, O. TI Seasonal and latitudinal variation of atmospheric methane: A ground-based and ship-borne solar IR spectroscopic study SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID ABSORPTION-SPECTROSCOPY; CARBON-MONOXIDE; TRACE GASES; EMISSIONS AB Column-averaged volume mixing ratios of CH(4) were retrieved with a precision of better than 0.5% from infrared solar absorption spectra obtained at Ny-Alesund ( Spitsbergen, 79 degrees N) between 1997 and 2004 and during two ship cruises (54 degrees N - 34 degrees S) on the Atlantic in 2003. The retrieval has been performed in a spectral region available to all operational FTIR ( Fourier Transform InfraRed) spectrometers performing solar absorption measurements. The seasonality and the long-term increase of the tropospheric volume-mixing ratio, derived from the infrared measurements agree well with data from surface sampling at this site. The latitudinal variation of ship-borne measurements between 54 degrees N and 34 degrees S is in agreement with inverse model simulations which are optimized vs. the global NOAA/ESRL measurements. C1 Univ Bremen, Inst Environm Phys, D-28359 Bremen, Germany. Inst Marine & Atmospher Res Utrecht, NL-3584 CC Utrecht, Netherlands. Commiss European Communities, Joint Res Ctr, I-21020 Ispra, Italy. Forschungszentrum Julich, D-52425 Julich, Germany. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. Royal Netherlands Meteorol Inst, NL-3730 AE De Bilt, Netherlands. Alfred Wegener Inst Polar & Marine Res, D-27570 Bremerhaven, Germany. RP Warneke, T (reprint author), Univ Bremen, Inst Environm Phys, Otto Hahn Allee 1, D-28359 Bremen, Germany. EM warneke@iup.physik.uni-bremen.de RI Velazco, Voltaire/H-2280-2011; GrooSS, Jens-Uwe/A-7315-2013; Notholt, Justus/P-4520-2016 OI Velazco, Voltaire/0000-0002-1376-438X; GrooSS, Jens-Uwe/0000-0002-9485-866X; Notholt, Justus/0000-0002-3324-885X NR 17 TC 12 Z9 12 U1 0 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 JUL 25 PY 2006 VL 33 IS 14 AR L14812 DI 10.1029/2006GL025874 PG 5 WC Geosciences, Multidisciplinary SC Geology GA 069ZK UT WOS:000239489000001 ER PT J AU Brooks, TF Humphreys, WM AF Brooks, TF Humphreys, WM TI A deconvolution approach for the mapping of acoustic sources (DAMAS) determined from phased microphone arrays SO JOURNAL OF SOUND AND VIBRATION LA English DT Article AB Current processing of acoustic array data is burdened with considerable uncertainty. This study reports an original methodology that serves to demystify array results, reduce misinterpretation, and accurately quantify position and strength of acoustic sources. Traditional array results represent noise sources that are convolved with array beamform response functions, which depend on array geometry, size (with respect to source position and distributions), and frequency. The Deconvolution Approach for the Mapping of Acoustic Sources (DAMAS) method removes beamforming characteristics from output presentations. A unique linear system of equations accounts for reciprocal influence at different locations over the array survey region. It makes no assumption beyond the traditional processing assumption of statistically independent noise sources. A new robust iterative method seamlessly introduces a positivity constraint (due to source independence) that makes the equation system sufficiently deterministic. DAMAS is quantitatively validated using archival data from a variety of prior high-lift airframe component noise studies, including flap edge/cove, trailing edge, leading edge, slat, and calibration sources. Presentations are explicit and straightforward, as the noise radiated from a region of interest is determined by simply summing the mean-squared values over that region. DAMAS can fully replace existing array processing and presentations methodology in most applications. It appears to dramatically increase the value of arrays to the field of experimental acoustics. Published by Elsevier Ltd. C1 NASA, Langley Res Ctr, Hampton, VA 23681 USA. RP Brooks, TF (reprint author), NASA, Langley Res Ctr, Hampton, VA 23681 USA. EM t.f.brooks@larc.nasa.gov NR 22 TC 114 Z9 127 U1 2 U2 16 PU ACADEMIC PRESS LTD ELSEVIER SCIENCE LTD PI LONDON PA 24-28 OVAL RD, LONDON NW1 7DX, ENGLAND SN 0022-460X J9 J SOUND VIB JI J. Sound Vibr. PD JUL 25 PY 2006 VL 294 IS 4-5 BP 856 EP 879 DI 10.1016/j.jsv.2005.12.046 PG 24 WC Acoustics; Engineering, Mechanical; Mechanics SC Acoustics; Engineering; Mechanics GA 054EI UT WOS:000238359200011 ER PT J AU Nikora, AP Munson, JC AF Nikora, Allen P. Munson, John C. TI Building high-quality software fault predictors SO SOFTWARE-PRACTICE & EXPERIENCE LA English DT Article; Proceedings Paper CT 28th Annual International Computer Software and Applications Conference CY SEP 28-30, 2004 CL Hong Kong, PEOPLES R CHINA DE software measurement; software fault modeling ID EVOLUTION AB Over the past several years, we have been developing software fault predictors based on a system's measured structural evolution. We have previously shown significant linear relationships between code churn, a set of synthesized metrics, and the rate at which faults are inserted into the system in terms of number of faults per unit change in code churn. A limiting factor in this and other such investigations has been the absence of a quantitative, consistent and repeatable definition of what constitutes a fault. The rules for fault definition were not sufficiently rigorous to provide unambiguous, repeatable fault counts. Within the framework of a space mission software development effort at the Jet Propulsion Laboratory we have developed a standard for the precise enumeration of faults. This new standard permits software faults to be measured directly from configuration control documents. We compared the new method of counting faults with two existing techniques to determine whether the fault-counting technique has an effect on the quality of the fault models constructed from those counts. The new fault definition provides higher quality fault models than those obtained using the other definitions of fault. Copyright (C) 2006 John Wiley & Sons, Ltd. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. Univ Idaho, Dept Comp Sci, Moscow, ID 83844 USA. RP Nikora, AP (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr,Mail Stop 125-233, Pasadena, CA 91109 USA. EM allen.p.nikora@jpl.nasa.gov NR 22 TC 4 Z9 4 U1 0 U2 0 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0038-0644 EI 1097-024X J9 SOFTWARE PRACT EXPER JI Softw.-Pract. Exp. PD JUL 25 PY 2006 VL 36 IS 9 BP 949 EP 969 DI 10.1002/spe.737 PG 21 WC Computer Science, Software Engineering SC Computer Science GA 068GR UT WOS:000239361500004 ER PT J AU Park, KB Ding, Y Pelz, JP Neudeck, PG Trunek, AJ AF Park, K. -B. Ding, Y. Pelz, J. P. Neudeck, P. G. Trunek, A. J. TI Valence band structure and band offset of 3C- and 4H-SiC studied by ballistic hole emission microscopy SO APPLIED PHYSICS LETTERS LA English DT Article ID HEXAGONAL SIC POLYTYPES; ELECTRONIC-PROPERTIES; 4H; POLARIZATION; LUMINESCENCE; INTERFACES; GROWTH; FIELD; 6H AB p-type Schottky barriers in Pt/3C-SiC contacts have been measured using ballistic hole emission microscopy (BHEM) and estimated to be similar to 0.06 eV higher than identically prepared Pt/p-type 4H-SiC contacts. This indicates the 3C-SiC valence band maximum (VBM) is similar to 0.06 eV below the 4H-SiC VBM, consistent with the calculated similar to 0.05 eV type-II valence band offset between these polytypes. We also observe no evidence of an additional VBM in 3C-SiC, which supports the proposal that the second VBM observed in BHEM spectra on 4H-SiC is a crystal-field split VBM located similar to 110 meV below the highest VBM. C1 Ohio State Univ, Dept Phys, Columbus, OH 43210 USA. NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. RP Park, KB (reprint author), Ohio State Univ, Dept Phys, 174 W 18th Ave, Columbus, OH 43210 USA. EM pelz.2@osu.edu RI Park, Kibog/F-5971-2010 OI Park, Kibog/0000-0003-4086-7365 NR 26 TC 6 Z9 7 U1 1 U2 8 PU AMER INST PHYSICS PI MELVILLE PA CIRCULATION & FULFILLMENT DIV, 2 HUNTINGTON QUADRANGLE, STE 1 N O 1, MELVILLE, NY 11747-4501 USA SN 0003-6951 J9 APPL PHYS LETT JI Appl. Phys. Lett. PD JUL 24 PY 2006 VL 89 IS 4 AR 042103 DI 10.1063/1.2218302 PG 3 WC Physics, Applied SC Physics GA 068LV UT WOS:000239376500057 ER EF